FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Rooker, JR
Wells, RJD
Itano, DG
Thorrold, SR
Lee, JM
AF Rooker, Jay R.
Wells, R. J. David
Itano, David G.
Thorrold, Simon R.
Lee, Jessica M.
TI Natal origin and population connectivity of bigeye and yellowfin tuna in
the Pacific Ocean
SO FISHERIES OCEANOGRAPHY
LA English
DT Article
DE equatorial Pacific; isotopes; migration; natal origin; otolith
chemistry; pelagic; stable isotopes; trace elements; stock mixing
ID ATLANTIC BLUEFIN TUNA; OTOLITH REFERENCE MATERIAL; STOCK FISHERY
COMPOSITION; THUNNUS-ALBACARES; ISOTOPE FRACTIONATION;
QUALITY-ASSURANCE; STABLE-ISOTOPES; MARINE FISH; SR-CA; MOVEMENTS
AB Natural chemical markers (stable isotopes and trace elements) in otoliths of bigeye tuna (Thunnus obesus) and yellowfin tuna (T.albacares) were used to investigate their origin and spatial histories in the western and central Pacific Ocean (WCPO). Otolith chemistry of young-of-the-year (YOY) T.obesus and T.albacares from four regions in the WCPO was first determined and used to establish baseline chemical signatures for each region. Spatial variation in stable isotope ratios of YOY T.obesus and T.albacares was detected, with the most noticeable difference being depleted otolith O-18 values for both species from the far west equatorial and west equatorial regions relative to the central equatorial and Hawaii regions. Elemental ratios in otoliths were also quantified for YOY T.obesus and T.albacares collected in 2008, and several showed promise for distinguishing YOY T.obesus (Mg:Ca, Mn:Ca, and Ba:Ca) and T.albacares (Li:Ca and Sr:Ca). The natal origin of age-1 to age-2+ T.obesus and T.albacares was then determined for two regions of the WCPO, and mixed-stock analysis indicated that T.obesus and T.albacares in our west equatorial sample were almost entirely from local production, with a minor contribution from central equatorial waters. Similarly, T. albacares collected in Hawaii were exclusively from local sources; however, a large fraction of T.obesus in Hawaii were classified to the central equatorial region, suggesting that the movement of migrants from outside production zones (i.e., south of Hawaii) are important to Hawaii's domestic fishery.
C1 [Rooker, Jay R.; Wells, R. J. David; Lee, Jessica M.] Texas A&M Univ, Dept Marine Biol, 1001 Texas Clipper Rd, Galveston, TX 77554 USA.
[Rooker, Jay R.; Wells, R. J. David] Texas A&M Univ, Dept Wildlife & Fisheries Sci, College Stn, TX 77843 USA.
[Itano, David G.] Natl Marine Fisheries Serv, Pacific Isl Reg, 1601 Kapiolani Blvd,Suite 1110, Honolulu, HI 96814 USA.
[Thorrold, Simon R.] Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA.
RP Rooker, JR (reprint author), Texas A&M Univ, Dept Marine Biol, 1001 Texas Clipper Rd, Galveston, TX 77554 USA.; Rooker, JR (reprint author), Texas A&M Univ, Dept Wildlife & Fisheries Sci, College Stn, TX 77843 USA.
EM rookerj@tamug.edu
RI Thorrold, Simon/B-7565-2012
OI Thorrold, Simon/0000-0002-1533-7517
FU University of Hawai'i Pelagic Fisheries Research Program (JIMAR project)
[651106]
FX Funding for this work was provided by the University of Hawai'i Pelagic
Fisheries Research Program (JIMAR project 651106 to JRR). A special
thanks to G. Castrence, P. Conley, J. Dettling, D. Dettman, B. Fukuda,
D. Fuller, E-J Kim, K. Lind, J. Muir, B. Muller, K. Pollock, K.
Schaefer, D. Secor, S. Tobiason, R. Wingate and T. Usu.
NR 66
TC 0
Z9 0
U1 3
U2 18
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1054-6006
EI 1365-2419
J9 FISH OCEANOGR
JI Fish Oceanogr.
PD MAY
PY 2016
VL 25
IS 3
BP 277
EP 291
DI 10.1111/fog.12154
PG 15
WC Fisheries; Oceanography
SC Fisheries; Oceanography
GA DJ0WE
UT WOS:000373924300006
ER
PT J
AU Keller, AA
Buchanan, JC
Steiner, E
Draper, D
Chappell, A
Frey, P
Head, MA
AF Keller, Aimee A.
Buchanan, John C.
Steiner, Erin
Draper, Doug
Chappell, Aaron
Frey, Peter
Head, Melissa A.
TI Size at maturity for grooved Tanner crab (Chionoecetes tanneri) along
the US west coast (Washington to California)
SO FISHERIES OCEANOGRAPHY
LA English
DT Article
DE abdominal width; allometric relationships; carapace width; chela length;
size at 50% maturity
ID EASTERN BERING-SEA; OPILIO BRACHYURA; SNOW CRAB; BIOLOGY; MAJIDAE;
GROWTH
AB We conducted a multiyear study to examine interannual variability in the mean size (carapace width, mm), maturity size (mm) and depth (m) for grooved Tanner crab (Chionoecetes tanneri (Rathbun, 1893)) along the U.S. west coast. An additional goal was to provide updated estimates of carapace width (mm) at 50% maturity (W-50) for male and female grooved Tanner crab and assess changes over time. Randomly selected samples came from trawl surveys undertaken annually by the Northwest Fisheries Science Center at depths of 55 to 1280m. We used allometric relationships between carapace width (CW) and either abdominal width (AW) (females) or chela length (CL) (males) to determine functional maturity by sex. We evaluated maturity by fitting logistic regression models to proportion mature grooved Tanner crab. W-50 varied significantly between males (125.2mm) and females (89.1mm) but interannual differences were slight. The annual mean CW were greater for mature males (139.9-143.4mm) relative to females (98.8-100.4mm). The average sizes of immature grooved Tanner crab varied between sexes with males (75.7-84.6mm) larger than females (66.7-71.9mm). Size frequency distributions indicated little overlap in the size of mature male and female grooved Tanner crab but considerable overlap between immature grooved Tanner crab. The best model expressing complexity in growth incorporated width, sex and maturity stage. Depth ranged from 195-1254m with the average depth of a mature grooved Tanner crab (females, 737m; males, 767m) significantly shallower than an immature (females, 949m; males, 918m) grooved Tanner crab.
C1 [Keller, Aimee A.; Steiner, Erin] Natl Ocean & Atmospher Adm, Fishery Resource Anal & Monitoring Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2725 Montlake Blvd East, Seattle, WA 98112 USA.
[Buchanan, John C.; Draper, Doug; Chappell, Aaron; Frey, Peter; Head, Melissa A.] Natl Ocean & Atmospher Adm, Fishery Resource Anal & Monitoring Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2032 S OSU Dr, Newport, OR 97365 USA.
RP Keller, AA (reprint author), Natl Ocean & Atmospher Adm, Fishery Resource Anal & Monitoring Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2725 Montlake Blvd East, Seattle, WA 98112 USA.
EM Aimee.Keller@noaa.gov
NR 37
TC 0
Z9 0
U1 2
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1054-6006
EI 1365-2419
J9 FISH OCEANOGR
JI Fish Oceanogr.
PD MAY
PY 2016
VL 25
IS 3
BP 292
EP 305
DI 10.1111/fog.12155
PG 14
WC Fisheries; Oceanography
SC Fisheries; Oceanography
GA DJ0WE
UT WOS:000373924300007
ER
PT J
AU Fortney, NW
He, S
Converse, BJ
Beard, BL
Johnson, CM
Boyd, ES
Roden, EE
AF Fortney, N. W.
He, S.
Converse, B. J.
Beard, B. L.
Johnson, C. M.
Boyd, E. S.
Roden, E. E.
TI Microbial Fe(III) oxide reduction potential in Chocolate Pots hot
spring, Yellowstone National Park
SO GEOBIOLOGY
LA English
DT Article
ID IRON ISOTOPE FRACTIONATION; SULFATE-REDUCING BACTERIA; STREAMER BIOFILM
COMMUNITIES; SOLE ELECTRON-ACCEPTOR; NOV SP-NOV; GEN. NOV.;
GEOBACTER-SULFURREDUCENS; DISSIMILATORY FE(III); DISSOLVED SULFIDE;
ELEMENTAL SULFUR
AB Chocolate Pots hot springs (CP) is a unique, circumneutral pH, iron-rich, geothermal feature in Yellowstone National Park. Prior research at CP has focused on photosynthetically driven Fe(II) oxidation as a model for mineralization of microbial mats and deposition of Archean banded iron formations. However, geochemical and stable Fe isotopic data have suggested that dissimilatory microbial iron reduction (DIR) may be active within CP deposits. In this study, the potential for microbial reduction of native CP Fe(III) oxides was investigated, using a combination of cultivation dependent and independent approaches, to assess the potential involvement of DIR in Fe redox cycling and associated stable Fe isotope fractionation in the CP hot springs. Endogenous microbial communities were able to reduce native CP Fe(III) oxides, as documented by most probable number enumerations and enrichment culture studies. Enrichment cultures demonstrated sustained DIR driven by oxidation of acetate, lactate, and H-2. Inhibitor studies and molecular analyses indicate that sulfate reduction did not contribute to observed rates of DIR in the enrichment cultures through abiotic reaction pathways. Enrichment cultures produced isotopically light Fe(II) during DIR relative to the bulk solid-phase Fe(III) oxides. Pyrosequencing of 16S rRNA genes from enrichment cultures showed dominant sequences closely affiliated with Geobacter metallireducens, a mesophilic Fe(III) oxide reducer. Shotgun metagenomic analysis of enrichment cultures confirmed the presence of a dominant G.metallireducens-like population and other less dominant populations from the phylum Ignavibacteriae, which appear to be capable of DIR. Gene (protein) searches revealed the presence of heat-shock proteins that may be involved in increased thermotolerance in the organisms present in the enrichments as well as porin-cytochrome complexes previously shown to be involved in extracellular electron transport. This analysis offers the firstdetailed insight into how DIR may impact the Fe geochemistry and isotope composition of a Fe-rich, circumneutral pH geothermal environment.
C1 [Fortney, N. W.; He, S.; Converse, B. J.; Beard, B. L.; Johnson, C. M.; Roden, E. E.] Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI USA.
[Boyd, E. S.] Montana State Univ, NASA, Astrobiol Inst, Dept Microbiol & Immunol, Bozeman, MT 59717 USA.
RP Roden, EE (reprint author), Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI USA.
EM eroden@geology.wisc.edu
FU NASA Astrobiology Institute
FX This work was supported by the NASA Astrobiology Institute. We thank H.
Xu (University of Wisconsin-Madison) for XRD analysis, and C. Gorski
(Pennsylvania State University) for Mossbauer analysis, of the CP
materials.
NR 111
TC 0
Z9 0
U1 19
U2 48
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1472-4677
EI 1472-4669
J9 GEOBIOLOGY
JI Geobiology
PD MAY
PY 2016
VL 14
IS 3
BP 255
EP 275
DI 10.1111/gbi.12173
PG 21
WC Biology; Environmental Sciences; Geosciences, Multidisciplinary
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Geology
GA DJ2UQ
UT WOS:000374061000004
PM 26750514
ER
PT J
AU Suhir, E
Ghaffarian, R
AF Suhir, E.
Ghaffarian, R.
TI Predicted stresses in a ball-grid-array (BGA)/column-grid-array (CGA)
assembly with an epoxy adhesive at its ends
SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS
LA English
DT Article
ID IDENTICAL NONDEFORMABLE ADHERENDS; INTERFACIAL THERMAL-STRESSES; BONDED
ASSEMBLIES; BONDING LAYER; STRAINS; JOINTS; SYSTEM; EDGE
AB A simple, easy-to-use and physically meaningful predictive model is suggested for the assessment of the thermal stresses in a ball-grid-array (BGA) or a column-grid-array (CGA) system with an epoxy adhesive at the peripheral portions of the assembly. It is shown that the application of such a design can lead to a considerable relief in the interfacial stress. The paper is a continuation and an extension of the recently published paper, in which a low modulus solder was considered for the peripheral portions of the assembly. The important difference is that while the soldering temperature has been assumed to be the same for the solder material throughout the assembly, the peripheral epoxy adhesive is applied at an appreciably lower (curing) temperature than the solder at the assembly's mid-portion. The numerical example has indicated that the application of the CGA technology enables one to achieve a 19.25 % stress relief in the case of an epoxy adhesive, while a 34.11 % stress relief could be expected in the case of a low modulus solder at the assembly ends. When a BGA technology is considered, the application of an epoxy or a low modulus solder at the peripheral portions of the assembly leads to the stress relief of about 14.42 % in the case of an epoxy and of about 12.80 % in the case of a low modulus solder. When CGA technology is used, the application of an epoxy at the peripheral portions of the assembly leads to about 8.70 % stress relief, while the application of a low modulus solder results in about 24.10 % relief. It is concluded that, with the yield stress in shear of 1.85 kgf/mm(2) for the solder in the assembly's mid-portion and 1.35 kgf/mm(2)-for the peripheral solder material, the application of the CGA technology in combination with an epoxy adhesive or a low modulus solder at the assembly ends might enable one to avoid inelastic strains in the solder, thereby increasing dramatically its fatigue lifetime, just because the low-cycle fatigue situation will be replaced in such a case with the elastic fatigue condition.
C1 [Suhir, E.] Portland State Univ, Portland, OR 97207 USA.
[Suhir, E.] Vienna Univ Technol, A-1060 Vienna, Austria.
[Suhir, E.] ERS Co, 727 Alvina Ct, Los Altos, CA 94024 USA.
[Ghaffarian, R.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Suhir, E (reprint author), Portland State Univ, Portland, OR 97207 USA.; Suhir, E (reprint author), Vienna Univ Technol, A-1060 Vienna, Austria.; Suhir, E (reprint author), ERS Co, 727 Alvina Ct, Los Altos, CA 94024 USA.
EM suhire@aol.com; reza.ghaffarian@jpl.nasa.gov
NR 65
TC 2
Z9 2
U1 3
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0957-4522
EI 1573-482X
J9 J MATER SCI-MATER EL
JI J. Mater. Sci.-Mater. Electron.
PD MAY
PY 2016
VL 27
IS 5
BP 4399
EP 4409
DI 10.1007/s10854-016-4310-2
PG 11
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA DI8HQ
UT WOS:000373742500033
ER
PT J
AU Lehnert, H
Stone, RP
AF Lehnert, Helmut
Stone, Robert P.
TI Two new species of sponges (Porifera, Demospongiae) from the Aleutian
Islands, Alaska
SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM
LA English
DT Article
DE new species; Megaciella; Cladocroce; Chalinidae; Acarnidae; Porifera;
Aleutian Islands; North Pacific
ID SP-NOV PORIFERA; USA; ASTROPHORIDA
AB Two new demosponges, Megaciella pituitosa and Cladocroce toxifera, are described from the Aleutian Islands, fostering our contention that the region is a hotspot of poriferan biodiversity. Seven of the thirteen species of Megaciella now known worldwide occur in the Sea of Okhotsk or around the Aleutian Islands. Similarly, five of the sixteen species of Cladocroce known worldwide occur in Alaska. Megaciella pituitosa sp. nov. possesses two categories of choanosomal styles and spicules of different sizes that differentiate it from all known congeners. Cladocroce toxifera sp. nov. differs from all known congeners by possessing toxa and an ectosomal tangential arrangement of oxeas.
C1 [Lehnert, Helmut] Eichenstr 14, D-86507 Oberottmarshausen, Germany.
[Lehnert, Helmut] Univ Munich, GeoBioCtr, Richard Wagner Str 10, D-80333 Munich, Germany.
[Stone, Robert P.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
RP Lehnert, H (reprint author), Eichenstr 14, D-86507 Oberottmarshausen, Germany.; Lehnert, H (reprint author), Univ Munich, GeoBioCtr, Richard Wagner Str 10, D-80333 Munich, Germany.
EM Lehnert@spongetaxonomics.de
FU Alaska Fisheries Science Center of NOAA/NMFS
FX Helmut Lehnert was supported by a contract from the Alaska Fisheries
Science Center of NOAA/NMFS.
NR 30
TC 1
Z9 1
U1 1
U2 3
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0025-3154
EI 1469-7769
J9 J MAR BIOL ASSOC UK
JI J. Mar. Biol. Assoc. U.K.
PD MAY
PY 2016
VL 26
IS 3
BP 673
EP 680
DI 10.1017/S0025315414001131
PG 8
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA DJ0UM
UT WOS:000373919900011
ER
PT J
AU Magar, KT
Balas, MJ
Frost, SA
AF Magar, Kaman Thapa
Balas, Mark J.
Frost, Susan A.
TI Direct adaptive torque control for maximizing the power captured by wind
turbine in partial loading condition
SO WIND ENERGY
LA English
DT Article
DE adaptive torque control; wind turbine control; wind speed estimation;
tip speed ratio tracking
AB In this paper, a direct adaptive control approach is used to track the tip speed ratio (TSR) of wind turbine to maximize the power captured during the below rated wind speed operation. Assuming a known optimum value of TSR, the deviation of actual TSR from the optimum one is mathematically expressed as TSR tracking error. Since the actual TSR is not a measurable quantity, this expression for TSR tracking error is linearized and simplified to express it in terms of wind speed and rotor speed, where rotor speed can easily be measured. Although it is possible to measure the wind speed with high accuracy using LiDAR, using it raises the overall cost of wind turbine installation; hence, a method to estimate the wind speed is also proposed. The adaptive controller operates on this simplified TSR tracking error to drive it to zero and to keep the TSR constant at desired optimum value. The performance of the proposed control scheme is illustrated by implementing and simulating it in the National Renewable Energy Laboratory 5MW wind turbine model and comparing the results with the existing baseline fixed gain controller. Copyright (c) 2015 John Wiley & Sons, Ltd.
C1 [Magar, Kaman Thapa; Balas, Mark J.] Embry Riddle Aeronaut Univ, Dept Aerosp Engn, Daytona Beach, FL 32114 USA.
[Frost, Susan A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Magar, KT (reprint author), Embry Riddle Aeronaut Univ, Dept Aerosp Engn, Daytona Beach, FL 32114 USA.
EM thapamak@erau.edu
NR 19
TC 1
Z9 1
U1 0
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1095-4244
EI 1099-1824
J9 WIND ENERGY
JI Wind Energy
PD MAY
PY 2016
VL 19
IS 5
BP 911
EP 922
DI 10.1002/we.1874
PG 12
WC Energy & Fuels; Engineering, Mechanical
SC Energy & Fuels; Engineering
GA DJ0XQ
UT WOS:000373928100008
ER
PT J
AU Hultquist, G
Graham, MJ
Smialek, JL
Kodra, O
AF Hultquist, G.
Graham, M. J.
Smialek, J. L.
Kodra, O.
TI Response to comment by A. Hedin et al. on "Corrosion of copper in
distilled water without oxygen and the detection of produced hydrogen"
SO CORROSION SCIENCE
LA English
DT Editorial Material
C1 [Hultquist, G.] Royal Inst Technol, Surface & Corros Sci, SE-10044 Stockholm, Sweden.
[Graham, M. J.] Natl Res Council Canada, Aerosp, Ottawa, ON K1A 0R6, Canada.
[Smialek, J. L.] NASA, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Kodra, O.] Natl Res Council Canada, Energy Min & Environm, Ottawa, ON K1A 0R6, Canada.
RP Graham, MJ (reprint author), Natl Res Council Canada, Aerosp, Ottawa, ON K1A 0R6, Canada.
EM mike.graham12@rogers.com
NR 11
TC 1
Z9 1
U1 2
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0010-938X
EI 1879-0496
J9 CORROS SCI
JI Corrosion Sci.
PD MAY
PY 2016
VL 106
BP 306
EP 307
DI 10.1016/j.corsci.2015.12.025
PG 2
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA DI8JZ
UT WOS:000373748600030
ER
PT J
AU Doerr, JC
Liu, H
Minello, TJ
AF Doerr, Jennifer C.
Liu, Hui
Minello, Thomas J.
TI Salinity Selection by Juvenile Brown Shrimp (Farfantepenaeus aztecus)
and White Shrimp (Litopenaeus setiferus) in a Gradient Tank
SO ESTUARIES AND COASTS
LA English
DT Article
DE Experimental tank; Farfantepenaeus aztecus; Litopenaeus setiferus;
Log-linear modeling; Penaeid shrimp; Salinity gradient
ID POSTLARVAL PENAEUS-AZTECUS; FLOW CHOICE CHAMBER; ESTUARINE ORGANISMS;
GROWTH; WATER; TEMPERATURE; PREFERENCE; PENAEIDAE; DECAPODA; SURVIVAL
AB Changes in freshwater inflow and salinity patterns may affect the nursery value of estuarine systems for penaeid shrimp, but the relationship between salinity and shrimp abundance is complex and likely confounded by other environmental variables. Laboratory experiments can provide insights into salinity selection, and we designed an experimental gradient tank to examine salinity preferences of juvenile brown shrimp and white shrimp. Our design uses gently flowing water to eliminate various physical constraints often associated with selection experiments. We conducted experiments with juvenile brown shrimp (12 trials) and white shrimp (seven trials), to examine selection for salinities along a gradient from 1 to 42. Data were analyzed using contingency tables and log-linear modeling to examine relationships with salinity and possible interactions with temperature. Both brown shrimp and white shrimp were present in all salinities examined within the experimental range. In general, brown shrimp showed a preference for salinities from 17 to 35 and demonstrated avoidance for the extreme low salinities along the gradient. Results for white shrimp were not statistically significant, and this species did not appear to avoid low salinities. There was no effect of water temperature on the observed selection patterns for brown or white shrimp. Our results suggest that although salinity preferences likely exist for these species, strong distribution trends associated with salinity gradients in estuaries are likely caused by other environmental factors.
C1 [Doerr, Jennifer C.; Minello, Thomas J.] NOAA, Galveston Lab, Natl Marine Fisheries Serv, SEFSC, 4700 Ave U, Galveston, TX 77551 USA.
[Liu, Hui] Texas A&M Univ, Dept Marine Biol, POB 1675, Galveston, TX 77553 USA.
RP Doerr, JC (reprint author), NOAA, Galveston Lab, Natl Marine Fisheries Serv, SEFSC, 4700 Ave U, Galveston, TX 77551 USA.
EM Jennifer.Doerr@noaa.gov
FU Northern Gulf Institute; National Marine Fisheries Service (NMFS)
Southeast Fisheries Science Center
FX Earlier designs of linear gradient tanks were built together with David
Aldrich, and we also thank him for discussions that improved our
experimental design. We thank Ronald Baker, Lauren Flynn, Shawn Hillen,
Juan Salas, and Elizabeth Wilson for assisting in data collection during
laboratory experiments and for numerous hours spent collecting shrimp in
the field. Lawrence Rozas provided comments that improved the original
version of this manuscript. We acknowledge the Northern Gulf Institute
and National Marine Fisheries Service (NMFS) Southeast Fisheries Science
Center for funding this research. The findings and conclusions in this
manuscript are those of the authors and do not necessarily represent the
views of NMFS.
NR 51
TC 0
Z9 0
U1 3
U2 4
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1559-2723
EI 1559-2731
J9 ESTUAR COAST
JI Estuaries Coasts
PD MAY
PY 2016
VL 39
IS 3
BP 829
EP 838
DI 10.1007/s12237-015-0019-3
PG 10
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA DI2WS
UT WOS:000373360500019
ER
PT J
AU Landsman, ZA
Licandro, J
Campins, H
Ziffer, J
de Pra, M
Cruikshank, DP
AF Landsman, Zoe A.
Licandro, Javier
Campins, Humberto
Ziffer, Julie
de Pra, Mario
Cruikshank, Dale P.
TI The Veritas and Themis asteroid families: 5-14 mu m spectra with the
Spitzer Space Telescope
SO ICARUS
LA English
DT Article
DE Asteroids; Asteroids composition; Asteroids surfaces; Infrared
observations; Spectroscopy
ID INFRARED SPECTROGRAPH IRS; SPECTROSCOPIC SURVEY; WATER-ICE; DUST;
ORGANICS; SURFACE; ORIGIN; MODEL; BELT; CHONDRITES
AB Spectroscopic investigations of primitive asteroid families constrain family evolution and composition and conditions in the solar nebula, and reveal information about past and present distributions of volatiles in the solar system. Visible and near-infrared studies of primitive asteroid families have shown spectral diversity between and within families. Here, we aim to better understand the composition and physical properties of two primitive families with vastly different ages: ancient Themis (similar to 2.5 Gyr) and young Veritas (similar to 8 Myr). We analyzed the 5 - 14 mu m Spitzer Space Telescope spectra of 11 Themis-family asteroids, including eight previously studied by Licandro et al. (2012), and nine Veritas-family asteroids, for a total of 20 asteroids in our sample. We detect a broad 10-mu m emission feature, attributed to fine-grained and/or porous silicate regolith, in all 11 Themis-family spectra and six of nine Veritas-family asteroids, with 10-mu m spectral contrast ranging from 1% +/- 0.1% to 8.5% +/- 0.9%. We used thermal modeling to derive diameters, beaming parameters and albedos for our sample. Asteroids in both families have beaming parameters near unity and geometric albedos in the range 0.03 - 0.14. Spectral contrast of the 10-mu m silicate emission feature is correlated with beaming parameter and rotation period in the Themis family, and may be related to near-infrared spectral slope for both families. We see no correlations of 10-mu m emission with diameter or albedo for either family. Comparison with laboratory spectra of primitive meteorites suggests these asteroids are similar to meteorites with relatively low abundances of phyllosilicates. Overall, our results suggest the Themis and Veritas families are primitive asteroids with variation in composition and/or regolith properties within both families. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Landsman, Zoe A.; Campins, Humberto] Univ Cent Florida, Dept Phys, 4111 Libra Dr,PS 430, Orlando, FL 32826 USA.
[Licandro, Javier] Inst Astrofis Canarias, C Via Lactea S-N, Tenerife 38205, Spain.
[Licandro, Javier] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Ziffer, Julie] Univ So Maine, Dept Phys, 96 Falmouth St, Portland, ME 04103 USA.
[de Pra, Mario] Observ Nacl, 77 Imperial Sao Cristovao, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Cruikshank, Dale P.] NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA.
RP Landsman, ZA (reprint author), Univ Cent Florida, Dept Phys, 4111 Libra Dr,PS 430, Orlando, FL 32826 USA.
EM zlandsman@knights.ucf.edu
FU Center for Lunar and Asteroid Surface Science (CLASS), a SSERVI team at
the University of Central Florida; NASA Florida Space Grant Consortium;
NASA's Near-Earth Object Observations program; MINECO, Spanish Ministry
of Economy and Competitiveness [ESP2013-47816-C4-2-P]
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. ZL and HC
acknowledge the support of the Center for Lunar and Asteroid Surface
Science (CLASS), a SSERVI team at the University of Central Florida. ZL
acknowledges the support of the NASA Florida Space Grant Consortium. HC
acknowledges support from NASA's Near-Earth Object Observations program.
JL acknowledges support from the Project ESP2013-47816-C4-2-P (MINECO,
Spanish Ministry of Economy and Competitiveness). This work benefited
from helpful comments from J. Emery and P. Vernazza. We especially thank
S. Fornasier for the insightful suggestions about beaming parameters and
rotation periods.
NR 45
TC 0
Z9 0
U1 0
U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAY 1
PY 2016
VL 269
BP 62
EP 74
DI 10.1016/j.icarus.2016.01.008
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI3QY
UT WOS:000373414800006
ER
PT J
AU Wiseman, SM
Arvidson, RE
Wolff, MJ
Smith, MD
Seelos, FP
Morgan, F
Murchie, SL
Mustard, JF
Morris, RV
Humm, D
McGuire, PC
AF Wiseman, S. M.
Arvidson, R. E.
Wolff, M. J.
Smith, M. D.
Seelos, F. P.
Morgan, F.
Murchie, S. L.
Mustard, J. F.
Morris, R. V.
Humm, D.
McGuire, P. C.
TI Characterization of artifacts introduced by the empirical volcano-scan
atmospheric correction commonly applied to CRISM and OMEGA near-infrared
spectra
SO ICARUS
LA English
DT Article
DE Mars; Mars, atmosphere; Mars, surface; Spectroscopy
ID MARS; ALGORITHM; EXPRESS
AB The empirical 'volcano-scan' atmospheric correction is widely applied to martian near infrared CRISM and OMEGA spectra between similar to 4000 and similar to 2600 nm to remove prominent atmospheric gas absorptions with minimal computational investment. This correction method employs division by a scaled empirically-derived atmospheric transmission spectrum that is generated from observations of the martian surface in which different path lengths through the atmosphere were measured and transmission calculated using the Beer-Lambert Law. Identifying and characterizing both artifacts and residual atmospheric features left by the volcano-scan correction is important for robust interpretation of CRISM and OMEGA volcano-scan corrected spectra. In order to identify and determine the cause of spectral artifacts introduced by the volcano-scan correction, we simulated this correction using a multiple scattering radiative transfer algorithm (DISORT). Simulated transmission spectra that are similar to actual CRISM-and OMEGA-derived transmission spectra were generated from modeled Olympus Mons base and summit spectra. Results from the simulations were used to investigate the validity of assumptions inherent in the volcano-scan correction and to identify artifacts introduced by this method of atmospheric correction. We found that the most prominent artifact, a bowl-shaped feature centered near 2000 nm, is caused by the inaccurate assumption that absorption coefficients of CO2 in the martian atmosphere are independent of column density. In addition, spectral albedo and slope are modified by atmospheric aerosols. Residual atmospheric contributions that are caused by variable amounts of dust aerosols, ice aerosols, and water vapor are characterized by the analysis of CRISM volcano-scan corrected spectra from the same location acquired at different times under variable atmospheric conditions. (C) 2016 Published by Elsevier Inc.
C1 [Wiseman, S. M.; Mustard, J. F.] Brown Univ, Dept Earth Environm & Planetary Sci, 324 Brook St,Box 1846, Providence, RI 02912 USA.
[Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
[Wolff, M. J.] Space Sci Inst, Boulder, CO USA.
[Smith, M. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Seelos, F. P.; Morgan, F.; Murchie, S. L.; McGuire, P. C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Morris, R. V.] NASA, Johnson Space Ctr, Houston, TX USA.
[Humm, D.] Space Instrument Calibrat Consulting, Annapolis, MD USA.
[McGuire, P. C.] Free Univ Berlin, Inst Geol Sci, Planetary Sci & Remote Sensing Grp, Berlin, Germany.
RP Wiseman, SM (reprint author), Brown Univ, Dept Earth Environm & Planetary Sci, 324 Brook St,Box 1846, Providence, RI 02912 USA.
EM sandra_wiseman@brown.edu
RI Murchie, Scott/E-8030-2015; Humm, David/B-8825-2016
OI Murchie, Scott/0000-0002-1616-8751; Humm, David/0000-0003-1520-261X
NR 23
TC 4
Z9 4
U1 3
U2 8
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAY 1
PY 2016
VL 269
BP 111
EP 121
DI 10.1016/j.icarus.2014.10.012
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI3QY
UT WOS:000373414800010
ER
PT J
AU Jain, A
Kuo, C
Sinkarenko, I
AF Jain, Abhinandan
Kuo, Calvin
Sinkarenko, Ivan
TI Feedforward dynamics for the control of articulated multi-limb robots
SO MULTIBODY SYSTEM DYNAMICS
LA English
DT Article; Proceedings Paper
CT 3rd Joint International Conference on Multibody System Dynamics (IMSD) /
7th Asian Conference on Multibody Dynamics (ACMD)
CY JUN 30-JUL 03, 2014
CL Busan, SOUTH KOREA
DE Robotics; Dynamics; Control
ID MANIPULATORS; STABILITY; MOTION
AB We describe a general approach for using linearizing feedforward control inputs for large degree of freedom (dof) multi-limb robots operating in scenarios involving motion and force constraints, and under-actuated degrees of freedom arising from the task and the environment. Our solution is general and has low computational cost needed for real-time control loops. It supports the tuning of the feedforward term to meet multiple task objectives. Being structure-based, it is able to easily accommodate changes in motion and force constraints that often occur in robotics scenarios.
C1 [Jain, Abhinandan; Kuo, Calvin; Sinkarenko, Ivan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jain@jpl.nasa.gov
NR 11
TC 0
Z9 0
U1 2
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1384-5640
EI 1573-272X
J9 MULTIBODY SYST DYN
JI Multibody Syst. Dyn.
PD MAY
PY 2016
VL 37
IS 1
BP 49
EP 68
DI 10.1007/s11044-016-9511-1
PG 20
WC Mechanics
SC Mechanics
GA DI6RQ
UT WOS:000373628100005
ER
PT J
AU Marrari, M
Piola, AR
Valla, D
Wilding, JG
AF Marrari, Marina
Piola, Alberto R.
Valla, Daniel
Wilding, John G.
TI Trends and variability in extended ocean color time series in the main
reproductive area of the Argentine hake, Merluccius hubbsi (Southwestern
Atlantic Ocean)
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Ocean color; SeaWiFS; MODIS; Time series; Merluccius hubbsi
ID CROSS-SHELF EXCHANGES; CHLOROPHYLL-A; CONTINENTAL-SHELF;
SURFACE-TEMPERATURE; SALINITY SIGNATURE; PATAGONIAN STOCK;
SOUTH-ATLANTIC; SEAWIFS; FRONTS; SEA
AB The Argentine hake Merluccius hubbsi is one of the main commercial resources of the Southwest Atlantic region, with a reported catch of 259,202 tons in 2014. Hake recruitment shows high interannual variability, yet the environmental and biological factors that influence reproduction are not fully understood. The increasing availability of ocean color data presents an opportunity to investigate a wide variety of fundamental topics including ocean primary productivity, climate change, and fisheries, among others. However, differences in the timing, length, and radiometer characteristics of the different missions result in a number of relatively short data records that are not suitable, individually, for the analysis of interdecadal changes. The combination of these datasets to produce longer time series of consistent data is essential for interpreting variability and trends in key parameters. We analyzed almost 5 years of high spatial resolution overlapping data from the SeaWiFS and MODIS Aqua sensors in the Southwestern Atlantic Ocean to assess differences in chlorophyll concentration retrievals, estimate uncertainties, and develop corrections. Data from SeaWiFS (1997-2006) and corrected MODIS (2007-2015) were analyzed jointly as a >17-year time series of consistent and continuous chlorophyll concentration data, the longest record to date in the region. Trend analyses performed in the main spawning and nursery areas of M. hubbsi revealed significant increases in chlorophyll concentrations since 1997. The environmental factors likely influencing the observed changes and the potential implications for recruitment of M. hubbsi are discussed. (C) 2016 The Authors. Published by Elsevier Inc.
C1 [Marrari, Marina; Piola, Alberto R.; Valla, Daniel] Serv Hidrog Naval, Dept Oceanog, Ave Montes de Oca 2124,C1270ABV, Buenos Aires, DF, Argentina.
[Marrari, Marina; Piola, Alberto R.; Valla, Daniel] Consejo Nacl Invest Cient & Tecn, Godoy Cruz 2290,C1425FQB, Buenos Aires, DF, Argentina.
[Marrari, Marina; Piola, Alberto R.; Valla, Daniel] Univ Buenos Aires, Inst Franco Argentino Estudios Clima & Sus Impact, Buenos Aires, DF, Argentina.
[Piola, Alberto R.; Valla, Daniel] Univ Buenos Aires, Fac Ciencias Exactas & Nat, Dept Ciencias Atmosfera & Oceanos, Buenos Aires, DF, Argentina.
[Wilding, John G.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Marrari, M (reprint author), Serv Hidrog Naval, Dept Oceanog, Ave Montes de Oca 2124,C1270ABV, Buenos Aires, DF, Argentina.
EM mmarrari@hidro.gov.ar
FU Fondo para la Investigation Cientifica y Tecnologica (Argentina)
[PICT-2013-1243, PICT-2012-0467]; Inter-American Institute for Global
Change Research through the US National Science Foundation [CRN3070,
GEO-1128040]
FX We thank B. Franz, J. Werdell, and C. Hu for their input comments. The
suggestions from two anonymous reviewers greatly improved this
manuscript. SeaWiFS and MODIS data were distributed by the NASA Ocean
Biology Processing Group. This study was partially funded by Fondo para
la Investigation Cientifica y Tecnologica (Argentina) grants
PICT-2013-1243 (MM), and PICT-2012-0467 (ARP). Additional funding was
provided by project CRN3070 from the Inter-American Institute for Global
Change Research through the US National Science Foundation grant
GEO-1128040.
NR 75
TC 0
Z9 0
U1 5
U2 13
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAY
PY 2016
VL 177
BP 1
EP 12
DI 10.1016/j.rse.2016.02.011
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DI5PC
UT WOS:000373550100001
ER
PT J
AU Alexandrov, MD
Cairns, B
Emde, C
Ackerman, AS
Ottaviani, M
Wasilewski, AP
AF Alexandrov, Mikhail D.
Cairns, Brian
Emde, Claudia
Ackerman, Andrew S.
Ottaviani, Matteo
Wasilewski, Andrzej P.
TI Derivation of cumulus cloud dimensions and shape from the airborne
measurements by the Research Scanning Polarimeter
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Cumulus clouds; Remote sensing; Cloud shape; Cloud dimensions
ID TOP HEIGHT; MISR; STEREO; RETRIEVAL; RECONSTRUCTION; GEOMETRY; IMPACT;
ASTER
AB The Research Scanning Polarimeter (RSP) is an airborne instrument, whose measurements have been extensively used for retrievals of microphysical properties of clouds. In this study we show that for cumulus clouds the information content of the RSP data can be extended by adding the macroscopic parameters of the cloud, such as its geometric shape, dimensions, and height above the ground. This extension is possible by virtue of the high angular resolution and high frequency of the RSP measurements, which allow for geometric constraint of the cloud's 2D cross section between a number of tangent lines of view. The retrieval method is tested on realistic 3D radiative transfer simulations and applied to actual RSP data. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Alexandrov, Mikhail D.] Columbia Univ, Dept Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA.
[Alexandrov, Mikhail D.; Cairns, Brian; Ackerman, Andrew S.; Ottaviani, Matteo; Wasilewski, Andrzej P.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Emde, Claudia] Univ Munich, Fak Phys, Meteorol Inst, Theresienstr 37, D-80333 Munich, Germany.
[Ottaviani, Matteo] CUNY City Coll, CREST, Dept Elect Engn, NOAA, 160 Convent Ave, New York, NY 10031 USA.
[Wasilewski, Andrzej P.] Trinnovim LLC, 2880 Broadway, New York, NY 10025 USA.
RP Alexandrov, MD (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA.
EM mda14@columbia.edu
RI Emde, Claudia/B-5447-2010;
OI Cairns, Brian/0000-0002-1980-1022
FU NASA Radiation Sciences Program; NASA HQ Science Mission
FX This research was supported by the NASA Radiation Sciences Program
managed by Hal Maring. We would like to acknowledge our gratitude to the
DEVOTE project team, the Research Services Directorate at NASA Langley
Research Center for supporting both King Air aircraft, and the HOPE
(Hands On Project Experience) Program co-funded though NASA HQ Science
Mission Directorate and Office of the Chief Engineer that enabled the
collection of the data used in this analysis. We would like to thank
four anonymous reviewers whose thoughtful comments helped us to
significantly improve the paper.
NR 31
TC 0
Z9 0
U1 1
U2 7
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAY
PY 2016
VL 177
BP 144
EP 152
DI 10.1016/j.rse.2016.02.032
PG 9
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DI5PC
UT WOS:000373550100012
ER
PT J
AU Ghods, M
Johnson, L
Lauer, M
Grugel, RN
Tewari, SN
Poirier, DR
AF Ghods, M.
Johnson, L.
Lauer, M.
Grugel, R. N.
Tewari, S. N.
Poirier, D. R.
TI Radial macrosegregation and dendrite clustering in directionally
solidified Al-7Si and Al-19Cu alloys
SO JOURNAL OF CRYSTAL GROWTH
LA English
DT Article
DE Directional solidification; Computer simulation; Fluid flows;
Segregation; Bridgman technique Aluminum alloys
ID AL-CU ALLOYS; NATURAL-CONVECTION; METALLIC ALLOYS; CRYSTAL-GROWTH;
BINARY-ALLOYS; SIMULATION; LIQUID; FLOW; CONSERVATION; INTERFACE
AB Hypoeutectic Al-7 wt% Si and Al-19 wt% Cu alloys were directionally solidified upward in a Bridgman furnace through a range of constant growth speeds and thermal gradients. Though processing is thermosolutally stable, flow initiated by gravity-independent advection at, slightly leading, central dendrites moves rejected solute out ahead and across the advancing interface. Here any lagging dendrites are further suppressed which promotes a curved solid-liquid interface and the eventual dendrite "clustering" seen in transverse sections (dendrite "steepling" in longitudinal orientations) as well as extensive radial macrosegregation. Both aluminum alloys showed considerable macrosegregation at the low growth speeds (10 and 30 mu m s(-1)) but not at higher speed (72 mu m s(-1)). Distribution of the fraction eutectic constituent on transverse sections was determined in order to quantitatively describe radial macro segregation. The convective mechanisms leading to dendrite-steepling were elucidated with numerical simulations, and their results compared with the experimental observations. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Ghods, M.; Johnson, L.; Tewari, S. N.] Cleveland State Univ, Chem & Biomed Engn Dept, Cleveland, OH 44115 USA.
[Lauer, M.; Poirier, D. R.] Univ Arizona, Dept Mat Sci & Engn, Tucson, AZ 85721 USA.
[Grugel, R. N.] NASA, Marshall Space Flight Space Ctr, Huntsville, AL 35811 USA.
[Johnson, L.] Cristal Corp, Ashtabula, OH 44004 USA.
[Lauer, M.] ME Elecmet Inc, Duluth, MN 55808 USA.
RP Ghods, M (reprint author), Cleveland State Univ, Chem & Biomed Engn Dept, Cleveland, OH 44115 USA.
EM ghods.masoud@gmail.com
FU NASA Grant [NX10AV4OG, NNX10AV40G]; Sandia National Laboratories Campus
Executive Fellowship Program
FX This work was supported by NASA Grant NX10AV4OG and NNX10AV40G. The
Al-7% Si alloys for our current research were kindly provided by Dr. Men
G. Chu at ALCOA Technical Center. M. Lauer would like to acknowledge
support from the Sandia National Laboratories Campus Executive
Fellowship Program. Acknowledgment of Prof. Sergio Felicelli at the
University of Akron and Prof. Juan Heinrich at the University of New
Mexico is needed for their two-decade effort in developing much of the
code used for this work.
NR 39
TC 2
Z9 2
U1 3
U2 17
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0248
EI 1873-5002
J9 J CRYST GROWTH
JI J. Cryst. Growth
PD MAY 1
PY 2016
VL 441
BP 107
EP 116
DI 10.1016/j.jcrysgro.2016.02.014
PG 10
WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied
SC Crystallography; Materials Science; Physics
GA DH4FT
UT WOS:000372741600017
ER
PT J
AU Bergmann, C
Barbour, J
LaForce, L
Driggers, WB
AF Bergmann, Charles
Barbour, James
LaForce, Lionel
Driggers, William B., III
TI Line cutter for use when releasing large marine organisms caught on
longline gear
SO FISHERIES RESEARCH
LA English
DT Article
DE Bycatch; Gangion; Line cutter; Monofilament; Prohibited species
AB Releasing large marine organisms captured on longline gear can often be difficult due to problems associated with the use of conventional line cutters. For example, struggling animals can remain below the water's surface for extended periods, thus providing limited access to the end of the leader nearest the hook. We describe a new line cutter design that outperforms conventional designs. The line cutter described herein can be deployed by a single individual and severs leader material in close proximity to the location of hooks while negating the need to bring the captured organism to the surface. The use of the line cutter reduces stress and potential injury to captured animals, is easily and inexpensively constructed, and has applications beyond its intended use, such as freeing lines snagged or entangled under vessels. Published by Elsevier B.V.
C1 [Bergmann, Charles; Barbour, James; LaForce, Lionel; Driggers, William B., III] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA.
RP Driggers, WB (reprint author), Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA.
EM william.driggers@noaa.gov
NR 5
TC 0
Z9 0
U1 1
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0165-7836
EI 1872-6763
J9 FISH RES
JI Fish Res.
PD MAY
PY 2016
VL 177
BP 124
EP 127
DI 10.1016/j.fishres.2016.01.018
PG 4
WC Fisheries
SC Fisheries
GA DG9BU
UT WOS:000372378600014
ER
PT J
AU Brown, LR
Nikitin, AV
Sung, K
Rey, M
Tashkun, SA
Tyuterev, VG
Crawford, TJ
Smith, MAH
Mantz, AW
AF Brown, L. R.
Nikitin, A. V.
Sung, K.
Rey, M.
Tashkun, S. A.
Tyuterev, Vl. G.
Crawford, T. J.
Smith, M. A. H.
Mantz, A. W.
TI Measurements and modeling of cold (CH4)-C-13 spectra in the 3750-4700
cm(-1) region
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Near infrared methane; Octad; FTIR; Cold spectra; Remote sensing
ID HIGH-RESOLUTION SPECTROSCOPY; DIPOLE-MOMENT SURFACES; MIRS COMPUTER
PACKAGE; MU-M; TETRAHEDRAL MOLECULES; ROVIBRATIONAL SPECTRA;
POLYATOMIC-MOLECULES; INTERACTING STATES; POTENTIAL-ENERGY;
INFRARED-SPECTRA
AB A new study of (CH4)-C-13 line intensities and positions was performed in the Octad region between 3750 and 4700 cm(-1). Using C-13-enriched samples, spectra were recorded with both the McMath-Pierce FTS at Kitt Peak Observatory in Arizona and the Bruker IFS-125HR at JPL. Sample temperatures ranged between 80 and 296 K. Line positions and intensities of similar to 15,000 features were retrieved at different temperatures by non-linear least squares curve-fitting procedures. Intensities were used to estimate the lower state energies for 60% of the features in order to determine quantum assignments up to J=10. A preliminary analysis was performed using the effective Hamiltonian and the effective dipole transition moment expressed in terms of irreducible tensor operators adapted to spherical top molecules. Selected assignments were made up to J=10 for all 24 sub-vibrational states of the Octad; these were modeled for 4752 experimental line positions and 3301 selected line intensities fitted with RMS standard deviations of 0.004 cm(-1) and 6.9%, respectively. Integrated intensities of the eight Octad bands are compared to ab initio variational calculations. A prediction of the (CH4)-C-13 is given, but further analysis to improve the calculation will be reported in the future. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Brown, L. R.; Sung, K.; Crawford, T. J.] CALTECH, Jet Prop Lab, Mailstop 200-105,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Nikitin, A. V.; Tashkun, S. A.] SB RAS, VE Zuev Inst Atmospher Opt, Lab Theoret Spect, 1 Academician Zuev Sq, Tomsk 634021, Russia.
[Nikitin, A. V.; Tashkun, S. A.] Tomsk State Univ, 36 Lenin Ave, Tomsk 634050, Russia.
[Rey, M.; Tyuterev, Vl. G.] Univ Reims, UFR Sci, UMR CNRS 7331, Grp Spectrometrie Mol & Atmospher, BP 1039, F-51687 Reims 2, France.
[Smith, M. A. H.] NASA Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
[Mantz, A. W.] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA.
RP Sung, K (reprint author), CALTECH, Jet Prop Lab, Mailstop 200-105,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM keeyoon.sung@jpl.nasa.gov
RI Tashkun, Sergey/E-8682-2014; Nikitin, Andrei/K-2624-2013; Sung,
Keeyoon/I-6533-2015
OI Nikitin, Andrei/0000-0002-4280-4096;
FU Tomsk State University Academic D.I. Mendeleev Fund Program grant; CNRS
(France); RFBR (Russia); IDRIS/CINES computer centre of France;
IDRIS/CINES computer centre Reims-Champagne-Ardenne
FX This study was supported by the Tomsk State University Academic D.I.
Mendeleev Fund Program grant. The support of the Laboratoire
International Associe SAMIA between CNRS (France) and RFBR (Russia),
from IDRIS/CINES computer centres of France and of the computer centre
Reims-Champagne-Ardenne is acknowledged. A.N. thanks Champagne-Ardenne
Region for the support and the computer centres of SKIF Siberia (Tomsk).
Part of the research described in this paper was performed at the Jet
Propulsion Laboratory, California Institute of Technology, Connecticut
College and the NASA Langley Research Center under contracts with the
National Aeronautics and Space Administration, including NASA's
Atmospheric Composition Laboratory Research (ACLR) program.
NR 60
TC 3
Z9 3
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAY
PY 2016
VL 174
BP 88
EP 100
DI 10.1016/j.jqsrt.2016.01.016
PG 13
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA DG9FU
UT WOS:000372389000010
ER
PT J
AU Jenerette, GD
Harlan, SL
Buyantuev, A
Stefanov, WL
Declet-Barreto, J
Ruddell, BL
Myint, SW
Kaplan, S
Li, XX
AF Jenerette, G. Darrel
Harlan, Sharon L.
Buyantuev, Alexander
Stefanov, William L.
Declet-Barreto, Juan
Ruddell, Benjamin L.
Myint, Soe Win
Kaplan, Shai
Li, Xiaoxiao
TI Micro-scale urban surface temperatures are related to land-cover
features and residential heat related health impacts in Phoenix, AZ USA
SO LANDSCAPE ECOLOGY
LA English
DT Article
DE Urban heat island; Parcel; MASTER; Land surface temperature; Social
surveys; Vulnerability
ID ECOSYSTEM SERVICES; UNITED-STATES; ISLAND; ARIZONA; NEIGHBORHOOD;
VEGETATION; MORTALITY; WATER; CONFIGURATION; VULNERABILITY
AB With rapidly expanding urban regions, the effects of land cover changes on urban surface temperatures and the consequences of these changes for human health are becoming progressively larger problems.
We investigated residential parcel and neighborhood scale variations in urban land surface temperature, land cover, and residents' perceptions of landscapes and heat illnesses in the subtropical desert city of Phoenix, AZ USA.
We conducted an airborne imaging campaign that acquired high resolution urban land surface temperature data (7 m/pixel) during the day and night. We performed a geographic overlay of these data with high resolution land cover maps, parcel boundaries, neighborhood boundaries, and a household survey.
Land cover composition, including percentages of vegetated, building, and road areas, and values for NDVI, and albedo, was correlated with residential parcel surface temperatures and the effects differed between day and night. Vegetation was more effective at cooling hotter neighborhoods. We found consistencies between heat risk factors in neighborhood environments and residents' perceptions of these factors. Symptoms of heat-related illness were correlated with parcel scale surface temperature patterns during the daytime but no corresponding relationship was observed with nighttime surface temperatures.
Residents' experiences of heat vulnerability were related to the daytime land surface thermal environment, which is influenced by micro-scale variation in land cover composition. These results provide a first look at parcel-scale causes and consequences of urban surface temperature variation and provide a critically needed perspective on heat vulnerability assessment studies conducted at much coarser scales.
C1 [Jenerette, G. Darrel] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA.
[Harlan, Sharon L.; Declet-Barreto, Juan] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ USA.
[Buyantuev, Alexander] SUNY Albany, Dept Geog & Planning, Albany, NY 12222 USA.
[Stefanov, William L.] NASA, Lyndon B Johnson Space Ctr, Explorat Integrat & Sci Directorate, Astromat Res & Explorat Sci Div, Houston, TX 77058 USA.
[Declet-Barreto, Juan] Nat Resources Def Council, Washington, DC USA.
[Ruddell, Benjamin L.] Arizona State Univ, Fulton Sch Engn, Tempe, AZ USA.
[Myint, Soe Win] Arizona State Univ, Sch Geog Sci & Urban Planning, Tempe, AZ USA.
[Kaplan, Shai] Ben Gurion Univ Negev, Jacob Blaustein Inst Desert Res, Beer Sheva, Israel.
[Li, Xiaoxiao] Arizona State Univ, Julie Ann Wrigley Global Inst Sustainabil, Tempe, AZ USA.
RP Jenerette, GD (reprint author), Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA.
EM darrel.jenerette@ucr.edu
OI Kaplan, Shai/0000-0003-1445-5244
FU National Science Foundation [GEO-0816168, GEO-0814692, BCS-1026865,
EF-1049251, EF-1049224, DEB-0919006]
FX This work was supported by National Science Foundation Grants
GEO-0816168, GEO-0814692, BCS-1026865, EF-1049251, EF-1049224, and
DEB-0919006. We thank Anthony Brazel and Chris Martin for their advice
on the MASTER data collection effort and David Hondoula for insightful
discussions. All data are available from CAP-LTER (caplter.asu.edu).
NR 70
TC 11
Z9 11
U1 14
U2 53
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0921-2973
EI 1572-9761
J9 LANDSCAPE ECOL
JI Landsc. Ecol.
PD MAY
PY 2016
VL 31
IS 4
BP 745
EP 760
DI 10.1007/s10980-015-0284-3
PG 16
WC Ecology; Geography, Physical; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Physical Geography; Geology
GA DG8FZ
UT WOS:000372319700005
ER
PT J
AU Zak, M
AF Zak, Michail
TI Non-Newtonian Aspects of Artificial Intelligence
SO FOUNDATIONS OF PHYSICS
LA English
DT Article
DE Randomness; Attractor; Stability
ID MODEL
AB The challenge of this work is to connect physics with the concept of intelligence. By intelligence we understand a capability to move from disorder to order without external resources, i.e., in violation of the second law of thermodynamics. The objective is to find such a mathematical object described by ODE that possesses such a capability. The proposed approach is based upon modification of the Madelung version of the Schrodinger equation by replacing the force following from quantum potential with non-conservative forces that link to the concept of information. A mathematical formalism suggests that a hypothetical intelligent particle, besides the capability to move against the second law of thermodynamics, acquires such properties like self-image, self-awareness, self-supervision, etc. that are typical for Livings. However since this particle being a quantum-classical hybrid acquires non-Newtonian and non-quantum properties, it does not belong to the physics matter as we know it: the modern physics should be complemented with the concept of the information force that represents a bridge to intelligent particle. As a follow-up of the proposed concept, the following question is addressed: can artificial intelligence (AI) system composed only of physical components compete with a human? The answer is proven to be negative if the AI system is based only on simulations, and positive if digital devices are included. It has been demonstrated that there exists such a quantum neural net that performs simulations combined with digital punctuations. The universality of this quantum-classical hybrid is in capability to violate the second law of thermodynamics by moving from disorder to order without external resources. This advanced capability is illustrated by examples. In conclusion, a mathematical machinery of the perception that is the fundamental part of a cognition process as well as intelligence is introduced and discussed.
C1 [Zak, Michail] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Zak, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM michail.zak@gmail.com
NR 11
TC 0
Z9 0
U1 4
U2 25
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0015-9018
EI 1572-9516
J9 FOUND PHYS
JI Found. Phys.
PD MAY
PY 2016
VL 46
IS 5
BP 517
EP 553
DI 10.1007/s10701-015-9977-3
PG 37
WC Physics, Multidisciplinary
SC Physics
GA DG8AG
UT WOS:000372304200001
ER
PT J
AU Weider, SZ
Nittler, LR
Murchie, SL
Peplowski, PN
Mccoy, TJ
Kerber, L
Klimczak, C
Ernst, CM
Goudge, TA
Starr, RD
Izenberg, NR
Klima, RL
Solomon, SC
AF Weider, Shoshana Z.
Nittler, Larry R.
Murchie, Scott L.
Peplowski, Patrick N.
Mccoy, Timothy J.
Kerber, Laura
Klimczak, Christian
Ernst, Carolyn M.
Goudge, Timothy A.
Starr, Richard D.
Izenberg, Noam R.
Klima, Rachel L.
Solomon, Sean C.
TI Evidence from MESSENGER for sulfur- and carbon-driven explosive
volcanism on Mercury
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID X-RAY SPECTROMETER; MAGMA VOLATILE CONTENT; SPECTRAL REFLECTANCE;
ERUPTION CONDITIONS; PLANETS FORMATION; IMPACT CRATERS; CALORIS BASIN;
MARINER 10; SURFACE; EVOLUTION
AB Targeted MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) X-Ray Spectrometer measurements of Mercury's largest identified pyroclastic deposit are combined with neutron and reflectance spectroscopy data to constrain the composition of volatiles involved in the eruption that emplaced the pyroclastic material. The deposit, northeast of the Rachmaninoff basin, is depleted in S (relative to Ca and Si) and C, compared with the rest of Mercury's surface. Spectral reflectance measurements of the deposit indicate relatively high overall reflectance and an oxygen-metal charge transfer (OMCT) absorption band at ultraviolet wavelengths. These results are consistent with oxidation of graphite and sulfides during magma ascent, via reaction with oxides in the magma or assimilated country rock, and the formation of S-and C-bearing volatile species. Consumption of graphite during oxidation could account for the elevated reflectance of the pyroclastic material, and the strength of the OMCT band is consistent with similar to 0.03-0.1 wt% FeO in the deposit.
C1 [Weider, Shoshana Z.; Nittler, Larry R.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
[Murchie, Scott L.; Peplowski, Patrick N.; Ernst, Carolyn M.; Izenberg, Noam R.; Klima, Rachel L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Mccoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
[Kerber, Laura] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Klimczak, Christian] Univ Georgia, Dept Geol, Athens, GA 30602 USA.
[Goudge, Timothy A.] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA.
[Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
RP Weider, SZ (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
EM sweider@carnegiescience.edu
RI Murchie, Scott/E-8030-2015; Ernst, Carolyn/I-4902-2012
OI Murchie, Scott/0000-0002-1616-8751;
FU NASA [NAS5-97271, NASW-00002]
FX We thank the MESSENGER engineering and instrument teams for the
successful operation of the MESSENGER spacecraft and payload. This work
is supported by the NASA Discovery Program under contracts NAS5-97271 to
The Johns Hopkins University Applied Physics Laboratory and NASW-00002
to the Carnegie Institution of Washington. We acknowledge Elizabeth
Frank, Ellen Crapster-Pregont, and Audrey Vorburger for analysis of the
global XRS data set, Malcolm Rutherford for insightful comments, as well
as Mikhail Zolotov and David Rothery for helpful reviews. All MESSENGER
data used in this paper are publicly available at the NASA Planetary
Data System.
NR 58
TC 2
Z9 2
U1 5
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 28
PY 2016
VL 43
IS 8
BP 3653
EP 3661
DI 10.1002/2016GL068325
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DP2RQ
UT WOS:000378338800005
ER
PT J
AU Mazloff, MR
Boening, C
AF Mazloff, Matthew R.
Boening, Carmen
TI Rapid variability of Antarctic Bottom Water transport into the Pacific
Ocean inferred from GRACE
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID OVERTURNING CIRCULATION; SEA; CLOSURE
AB Air-ice-ocean interactions in the Antarctic lead to formation of the densest waters on Earth. These waters convect and spread to fill the global abyssal oceans. The heat and carbon storage capacity of these water masses, combined with their abyssal residence times that often exceed centuries, makes this circulation pathway the most efficient sequestering mechanism on Earth. Yet monitoring this pathway has proven challenging due to the nature of the formation processes and the depth of the circulation. The Gravity Recovery and Climate Experiment (GRACE) gravity mission is providing a time series of ocean mass redistribution and offers a transformative view of the abyssal circulation. Here we use the GRACE measurements to infer, for the first time, a 2003-2014 time series of Antarctic Bottom Water export into the South Pacific. We find this export highly variable, with a standard deviation of 1.87 sverdrup (Sv) and a decorrelation timescale of less than 1 month. A significant trend is undetectable.
C1 [Mazloff, Matthew R.] Univ Calif San Diego, Scripps Inst Oceanog, Dept Climate Atmospher Sci & Phys Oceanog, La Jolla, CA 92093 USA.
[Boening, Carmen] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Mazloff, MR (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Dept Climate Atmospher Sci & Phys Oceanog, La Jolla, CA 92093 USA.
EM mmazloff@ucsd.edu
FU National Science Foundation (NSF) [OCE-1234473, PLR-1425989]; National
Science Foundation [MCA06N007]; NASA
FX We would like to thank three anonymous reviewers for their feedback that
improved this manuscript. M.M. acknowledges the National Science
Foundation (NSF) for support of this research through grants OCE-1234473
and PLR-1425989. SOSE was produced using the Extreme Science and
Engineering Discovery Environment (XSEDE), which is supported by
National Science Foundation grant MCA06N007. The work has been partially
performed at the Jet Propulsion Laboratory/California Institute of
Technology. This research was partially supported by NASA funding for
the GRACE mission. We would like to thank Michael Watkins, David Wiese,
and Dah-Ning Yuan for the processing of the GRACE mascon data.
NR 28
TC 1
Z9 1
U1 4
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 28
PY 2016
VL 43
IS 8
BP 3822
EP 3829
DI 10.1002/2016GL068474
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DP2RQ
UT WOS:000378338800026
ER
PT J
AU Lee, T
AF Lee, Tong
TI Consistency of Aquarius sea surface salinity with Argo products on
various spatial and temporal scales
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; INSTABILITY WAVES; INDIAN-OCEAN; SMOS;
SATELLITE; IMPACT; VALIDATION; ERROR
AB Understanding the accuracies of satellite-derived sea surface salinity measurements in depicting temporal changes and their dependence on spatiotemporal scales is important to applications, capability assessment, and future satellite mission design. This study quantifies the consistency between Aquarius Version 4 monthly gridded sea surface salinity (SSS) with two Argo-based monthly gridded near-surface salinity products for describing temporal changes on 1 degrees x 1 degrees, 3 degrees x 3 degrees, and 10 degrees x 10 degrees scales. Globally averaged standard deviation values for Aquarius-Argo salinity differences on these three spatial scales are 0.16, 0.14, and 0.09 practical salinity unit (psu), compared to those between the two Argo products of 0.10, 0.09, and 0.04 psu. The consistency between Aquarius and Argo is similar to that between the two Argo products in the tropics for seasonal signals, and in the tropics and midlatitudes for nonseasonal signals. Therefore, the uncertainties of Argo products for various scales need to be considered in evaluating satellite SSS. Innovative satellite technologies are needed to improve high-latitude satellite SSS measurements.
C1 [Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Lee, T (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM tlee@jpl.nasa.gov
FU NASA Physical Oceanography Program; NASA; California Institute of
Technology, Government
FX This research was carried out at the Jet Propulsion Laboratory (JPL),
California Institute of Technology, under a contract with NASA,
supported by NASA Physical Oceanography Program. The data sets used in
the analysis were downloaded from:
ftp://podaac-ftp.jpl.nasa.gov/SalinityDensity/aquarius/L3/mapped/V4/mont
hly/SCISM/ (Aquarius Version 4),
http://www.argo.ucsd.edu/Gridded_fields.html (Argo-SIO), and
http://apdrc.soest.hawaii.edu/projects/Argo/data/gridded/On_standard_lev
els/index-1.html (ArgoUH). The author also thanks the two anonymous
reviewers for their constructive comments. Copyright 2016 California
Institute of Technology, Government sponsorship acknowledged.
NR 33
TC 0
Z9 0
U1 4
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 28
PY 2016
VL 43
IS 8
BP 3857
EP 3864
DI 10.1002/2016GL068822
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DP2RQ
UT WOS:000378338800030
ER
PT J
AU de Wit, RJ
Janches, D
Fritts, DC
Hibbins, RE
AF de Wit, R. J.
Janches, D.
Fritts, D. C.
Hibbins, R. E.
TI QBO modulation of the mesopause gravity wave momentum flux over Tierra
del Fuego
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID QUASI-BIENNIAL OSCILLATION; MIDDLE ATMOSPHERE; SOUTHERN-HEMISPHERE;
MODEL; CIRCULATION; WINDS
AB The interannual variability of the mesosphere and lower thermosphere (MLT) gravity wave momentum flux over southern midlatitudes (53.7 degrees S) has been studied using more than 7 years of meteor radar observations at Rio Grande, Argentina. A modulation, with periods similar to that of the equatorial stratospheric quasi-biennial oscillation (QBO), is observed in the vertical flux of zonal as well as meridional momentum. The QBO signal is largest in the zonal component during summer and is in phase with the stratospheric QBO at 50 hPa (similar to 21 km). The relation between the stratospheric QBO and the QBO modulation in the MLT gravity wave forcing (derived from the divergence of the momentum flux) was found to be consistent with that expected from the Holton-Tan effect coupled to the interhemispheric coupling mechanism. These results provide the first observational support for the existence of the midlatitude gravity wave forcing anomalies as hypothesized in the interhemispheric coupling mechanism.
C1 [de Wit, R. J.; Janches, D.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Fritts, D. C.] GATS Inc, Boulder, CO USA.
[Hibbins, R. E.] NTNU, Dept Phys, Trondheim, Norway.
[Hibbins, R. E.] Birkeland Ctr Space Sci, Bergen, Norway.
RP de Wit, RJ (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM rosmarie.j.dewit@nasa.gov
RI Janches, Diego/D-4674-2012
OI Janches, Diego/0000-0001-8615-5166
FU NSF [AGS-1112830]; NASA; Research Council of Norway/CoE [223252/F50]
FX Helpful discussions with Patrick Espy are gratefully acknowledged. In
addition, we wish to thank the Estacion Astronomica Rio Grande (EARG)
personnel for their invaluable help with the operation of SAAMER. SAAMER
is supported by NSF under grant AGS-1112830. This work was supported by
RJW's appointment to the NASA Postdoctoral Program, administered by
Universities Space Research Association through a contract with NASA,
and in part by the Research Council of Norway/CoE under contract
223252/F50 (REH). Singapore radiosonde data are available from the Free
University of Berlin, and meteor radar data are available from the
authors upon request.
NR 33
TC 0
Z9 0
U1 4
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 28
PY 2016
VL 43
IS 8
BP 4049
EP 4055
DI 10.1002/2016GL068599
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DP2RQ
UT WOS:000378338800053
ER
PT J
AU Bergman, JW
Jensen, EJ
Pfister, L
Bui, TV
AF Bergman, John W.
Jensen, Eric J.
Pfister, Leonhard
Bui, Thaopaul V.
TI Air parcel trajectory dispersion near the tropical tropopause
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID STRATOSPHERIC WATER-VAPOR; 2-DIMENSIONAL TURBULENCE; AIRCRAFT
OBSERVATIONS; MODEL EVALUATION; LAYER; TRANSPORT; OZONE; DEHYDRATION;
CONVECTION; FORECASTS
AB Dispersion of backward air parcel trajectories that are initially tightly grouped near the tropical tropopause is examined using three ensemble approaches: "RANWIND," in which different ensemble members use identical resolved wind fluctuations but different realizations of stochastic, multifractal simulations of unresolved winds; "PERTLOC," in which members use identical resolved wind fields but initial locations are perturbed 2 degrees in latitude and longitude; and a multimodel ensemble ("MULTIMODEL") that uses identical initial conditions but different resolved wind fields and/or trajectory formulations. Comparisons among the approaches distinguish, to some degree, physical dispersion from that due to data uncertainty and the impacts of unresolved wind fluctuations from those of resolved variability. Dispersion rates are robust properties of trajectories near the tropical tropopause. Horizontal dispersion rates are typically similar to 3 degrees/d, which is large enough to spread parcels throughout the tropics within typical tropical tropopause layer transport times (30-60 days) and underscores the importance of averaging large collections of trajectories to obtain reliable parcel source and pathway distributions. Vertical dispersion rates away from convection are similar to 2-3 hPa/d. Dispersion is primarily carried out by the resolved flow, and the RANWIND approach provides a plausible representation of actual trajectory dispersion rates, while PERTLOC provides a reasonable and inexpensive alternative to RANWIND. In contrast, dispersion from the MULTIMODEL calculations is important because it reflects systematic differences in resolved wind fields from different reanalysis data sets.
C1 [Bergman, John W.] Bay Area Environm Res Inst, Petaluma, CA USA.
[Bergman, John W.] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
[Jensen, Eric J.; Pfister, Leonhard; Bui, Thaopaul V.] NASA Ames Res Ctr, Earth Sci Div, Moffett Field, CA USA.
RP Bergman, JW (reprint author), Bay Area Environm Res Inst, Petaluma, CA USA.; Bergman, JW (reprint author), Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
EM j.w.bergman921@gmail.com
FU National Science Foundation
FX The tenor of this study owes much to enlightening discussions with J.
Barsugli, C. Penland, and P. Sardeshmukh. We are also grateful for the
thoughtful comments of three anonymous reviewers. ECMWF operational
analysis, ERA-interim, CFSR, and GSF data were obtained from the CISL
Data Support Section at the National Center for Atmospheric Research
(NCAR). MERRA, TRMM, and IR data were obtained from the Goddard Earth
Sciences Data and Information Services Center. The Yang et al. [2010]
radiative heating rate data were provided by Q. Yang. J. Bergman and E.
Jensen were visitors at the Atmospheric Chemistry Observations and
Modeling Laboratory of NCAR during the execution of this study. The
National Center for Atmospheric Research is operated by the University
Corporation for Atmospheric Research, under sponsorship of the National
Science Foundation. Data used in this study can be obtained free of
charge by contacting J. Bergman (jwbergman921@gmail.com).
NR 58
TC 0
Z9 0
U1 7
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2016
VL 121
IS 8
BP 3759
EP 3775
DI 10.1002/2015JD024320
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP2KU
UT WOS:000378318100002
ER
PT J
AU Mace, GG
Avey, S
Cooper, S
Lebsock, M
Tanelli, S
Dobrowalski, G
AF Mace, Gerald G.
Avey, Stephanie
Cooper, Steven
Lebsock, Matthew
Tanelli, Simone
Dobrowalski, Greg
TI Retrieving co-occurring cloud and precipitation properties of warm
marine boundary layer clouds with A-Train data
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID DROPLET EFFECTIVE RADIUS; VERTICAL VARIATION; RADAR; MODEL;
PARAMETERIZATION; STRATOCUMULUS; MICROPHYSICS; ORGANIZATION;
PERFORMANCE; RADIOMETER
AB In marine boundary layer (MBL) clouds the formation of precipitation from the cloud droplet distribution in the presence of variable aerosol plays a fundamental role in determining the coupling of these clouds to their environment and ultimately to the climate system. Here the degree to which A-Train satellite measurements can diagnose simultaneously occurring cloud and precipitation properties in MBL clouds is examined. Beginning with the measurements provided by CloudSat and Moderate Resolution Imaging Spectroradiometer (including a newly available microwave brightness temperature from CloudSat), and a climatology of MBL cloud properties from past field campaigns, an assumption is made that any hydrometeor volume could contain both cloud droplet and precipitation droplet modes. Bayesian optimal estimation is then used to derive atmospheric states by inverting a measurement vector carefully accounting for uncertainties due to instrument noise, forward model error, and assumptions. It is found that in many cases where significant precipitation coexists with cloud, due to forward model error driven by uncertainties in assumptions, the uncertainty in retrieved cloud properties is greater than the variance in the prior climatology. It is often necessary to average several thousand (hundred) precipitating (weakly precipitating) profiles to obtain meaningful information regarding the properties important to microphysical processes. Regardless, if such process level information is deemed necessary for better constraining predictive models of the climate system, measurement systems specifically designed to accomplish such retrievals must be considered for the future.
C1 [Mace, Gerald G.; Avey, Stephanie; Cooper, Steven] Univ Utah, Dept Atmospher Sci, Salt Lake City, UT USA.
[Lebsock, Matthew; Tanelli, Simone; Dobrowalski, Greg] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Mace, GG (reprint author), Univ Utah, Dept Atmospher Sci, Salt Lake City, UT USA.
EM jay.mace@utah.edu
FU NASA [NNX10AM42G, NNX15AK17G, NNX13A169G]
FX CloudSat, MODIS, and all meteorological data used in completion of this
work were acquired from the CloudSat Data Processing Center at the
Colorado State University (http://www.cloudsat.cira.colostate.edu). Data
from the field programs MASE I and MASE II were kindly provided by Armin
Sorooshian at armin@email.arizona.edu. RICO data were acquired from
http://data.eol.ucar.edu/master_list/?project=RICO. TC4 data were
acquired from https://espo.nasa.gov. We acknowledge the efforts of the
engineers and scientists at the Jet Propulsion Laboratory, Ball
Aerospace, and the Cooperative Institute for Research in the Atmosphere
(CIRA) at the Colorado State University without whom the CloudSat
project would not be successful. We acknowledge the efforts of several
anonymous reviewers and Dave Turner whose efforts resulted in a greatly
improved manuscript. G.M., S.A., and S.C. acknowledge support under NASA
grants NNX10AM42G, NNX15AK17G, and NNX13A169G. Part of the research
described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 60
TC 4
Z9 4
U1 5
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2016
VL 121
IS 8
BP 4008
EP 4033
DI 10.1002/2015JD023681
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP2KU
UT WOS:000378318100016
ER
PT J
AU Chronis, T
Koshak, W
McCaul, E
AF Chronis, T.
Koshak, W.
McCaul, E.
TI Why do oceanic negative cloud-to-ground lightning exhibit larger peak
current values?
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CONTINENTAL UNITED-STATES; DIURNAL-VARIATION; CHARGE-TRANSFER; RETURN
STROKES; ICE NUCLEATION; SPACE-CHARGE; SEA; ELECTRIFICATION; PARTICLES;
NLDN
AB This study examines the temporal (monthly) and spatial climatology (2004-2010) of the first return stroke of the cloud-to-ground (CG) lightning flash peak current (I-p) across various land/water boundaries over the contiguous United States. Four regions are examined: the Gulf of Mexico (region 1), the Florida peninsula (region 2), Lake Michigan (region 3), and part of the U.S. Mid-Atlantic (region 4). The cross sections across the coastlines of regions 1, 2, and 4 show a gradual oceanward increase in the mean negative polarity CG peak current values (-I-p). This transition along the respective land/ocean boundaries is not sharp but gradual. In direct contrast with ocean, there is no consistent behavior in -I-p values as we move from land out across the fresh water of Lake Michigan (region 3). Meanwhile, the positive CG flash peak current (+I-p) values do not exhibit a consistent variation across any coastal boundary. For region 1, the -I-p values increase as we move toward the coast (southwards) especially during the wet season (June-October). This finding is in direct contrast with studies that documented winter as the season of maximum -I-p values. The zonal and seasonal variations of -I-p values across region 4 are not quite as pronounced, but the oceanic -I-p values are still larger than over the adjoining landmass. We explore in turn which up to date hypotheses pertinent to the oceanic -I-p enhancement are supported or refuted by our findings. It is concluded that the oceanic -I-p enhancement is not an artifact related to CG detection or -I-p retrieval methods, nor is it likely related to the cloud top heights or CG activity. The study cannot refute the role of electrical conductivity and its contribution to CG leader attachment processes. However, given the observed "blurred transition" of the I-p values across the coastlines this paper suggests that likely the main physical mechanism is acting on the thundercloud potential. The recently suggested role of sodium chloride (NaCl) but also the role of ice crystal size (implicated herein), as possible modulators of the thundercloud potential, exhibit distinct pros and cons. Their candidacy is supported by their strong physical links to the electrostatic charging and thundercloud electric potential buildup but also by the exhibited blurred -I-p transition across the coastlines. In contrast, the suggested mechanisms cannot individually explain the observed -I-p enhancement in terms of season, NaCl concentrations, and absence of similar behavior in the respective +I-p values.
C1 [Chronis, T.] Univ Alabama, Earth Syst Sci Ctr, Huntsville, AL 35899 USA.
[Koshak, W.] NASA Marshall Space Flight Ctr, Earth Sci Off, ZP11, Huntsville, AL USA.
[McCaul, E.] Univ Space Res Assoc, Huntsvillle, AL USA.
RP Chronis, T (reprint author), Univ Alabama, Earth Syst Sci Ctr, Huntsville, AL 35899 USA.
EM themis.chronis@nsstc.uah.edu
FU GOES-R System Program as part of the Proving Ground and Risk Reduction
programs
FX The first author acknowledges the support by Steve Goodman and the
GOES-R System Program as part of the Proving Ground and Risk Reduction
programs. The authors greatly appreciate the comments by Earle Williams
and Ken Cummins. We also extend our thanks to Ryan Said, Ted Mansell,
Walter Lyons, and George Chronis for their input. The NLDN data were
kindly provided by Vaisala Inc. through a UAH/ESSC memorandum of
agreement, for research purposes only. The NLDN data are available at
http://thunderstorm.vaisala.com.
NR 85
TC 2
Z9 2
U1 2
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2016
VL 121
IS 8
BP 4049
EP 4068
DI 10.1002/2015JD024129
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP2KU
UT WOS:000378318100018
ER
PT J
AU Lu, GP
Cummer, SA
Tian, Y
Zhang, HB
Lyu, FC
Wang, T
Stanley, MA
Yang, J
Lyons, WA
AF Lu, Gaopeng
Cummer, Steven A.
Tian, Ye
Zhang, Hongbo
Lyu, Fanchao
Wang, Tao
Stanley, Mark A.
Yang, Jing
Lyons, Walter A.
TI Sprite produced by consecutive impulse charge transfers following a
negative stroke: Observation and simulation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LIGHTNING DISCHARGES; MOMENT CHANGES; ELF RADIATION; CURRENTS;
IONOSPHERE; TRANSIENTS; MORPHOLOGY; MECHANISM; FLORIDA; PULSES
AB On the morning of 5 June 2013, two cameras of the SpriteCam network concurrently captured a red sprite with diffuse halo over a mesoscale convective system (MCS) passing the panhandle area of Oklahoma. This sprite was produced by a negative cloud-to-ground (CG) stroke with peak current of -103 kA in a manner different from previous observations in several aspects. First of all, the causative stroke of sprite is located by the National Lightning Detection Network (NLDN) in the trailing stratiform of MCS, instead of the deep convection typically for negative sprites. Second, the sprite-producing stroke was likely the first stroke of a multistroke negative CG flash (with >= 6 CG strokes) whose evolution was mainly confined in the lower part of thunderstorm; although the parent flash of sprite might contain relatively long in-cloud evolution prior to the first stroke, there is no evidence that the negative leader had propagated into the upper positive region of thundercloud as typically observed for the sprite-producing/class negative CG strokes. Third, as shown by the simulation with a two-dimensional full-wave electrodynamic model, although the impulse charge moment change (-190 C km) produced by the main stroke was not sufficient to induce conventional breakdown in the mesosphere, a second impulse charge transfer occurred with similar to 2 ms delay to cause a substantial charge transfer (-290 C km) so that the overall charge moment change (-480 C km) exceeded the threshold for sprite production; this is a scenario different from the typical case discussed by Li et al. (2012). As for the source of the second current pulse that played a critical role to produce the sprite, it could be an M component whose charge source was at least 9 km horizontally displaced from the main stroke or a negative CG stroke (with weak peak current for the return stroke) that was not detected by the NLDN.
C1 [Lu, Gaopeng; Tian, Ye; Zhang, Hongbo; Yang, Jing] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing, Peoples R China.
[Lu, Gaopeng; Yang, Jing] Nanjing Univ Informat Sci & Technol, Collaborat Innovat Ctr Forecast & Evaluat Meteoro, Nanjing, Jiangsu, Peoples R China.
[Lu, Gaopeng] Nanjing Univ Informat Sci & Technol, Key Lab Meteorol Disaster, Minist Educ, Nanjing, Jiangsu, Peoples R China.
[Cummer, Steven A.; Lyu, Fanchao] Duke Univ, Elect & Comp Engn Dept, Durham, NC USA.
[Tian, Ye; Zhang, Hongbo] Univ Chinese Acad Sci, Beijing, Peoples R China.
[Wang, Tao] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA.
[Wang, Tao] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Stanley, Mark A.] New Mexico Inst Min & Technol, Langmuir Lab, Socorro, NM 87801 USA.
[Lyons, Walter A.] FMA Res, Ft Collins, CO USA.
RP Lu, GP (reprint author), Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing, Peoples R China.; Lu, GP (reprint author), Nanjing Univ Informat Sci & Technol, Collaborat Innovat Ctr Forecast & Evaluat Meteoro, Nanjing, Jiangsu, Peoples R China.; Lu, GP (reprint author), Nanjing Univ Informat Sci & Technol, Key Lab Meteorol Disaster, Minist Educ, Nanjing, Jiangsu, Peoples R China.
EM gaopenglu@gmail.com
RI ZHANG, Hongbo/S-7439-2016; Wang, Tao/C-2381-2011
OI ZHANG, Hongbo/0000-0003-0673-9482; Wang, Tao/0000-0003-3430-8508
FU National Key Basic Research and Development Program (973) of China
[2014CB441405]; Natural Science Foundation of China [41574179]; Open
Research Program of Key Laboratory of Meteorological Disaster (Nanjing
University of Information Science and Technology) of Ministry of
Education [KLME1414]; Chinese Academy of Sciences [2013068]; DARPA
Nimbus program
FX This work was supported by National Key Basic Research and Development
Program (973) of China (2014CB441405), Natural Science Foundation of
China (41574179), Open Research Program of Key Laboratory of
Meteorological Disaster (Nanjing University of Information Science and
Technology) of Ministry of Education (KLME1414), and "The Hundred
Talents Program" of Chinese Academy of Sciences (2013068). Kevin Palivec
is acknowledged for running sprite observations from Hawley, Texas. We
thank Bill Rison (New Mexico Tech), William Beasley (University of
Oklahoma), and Eric Brunning (Texas Tech University) for inspiring
discussions on the possible detection of VHF sources from the
sprite-producing flash. The observations reported in this paper were
obtained with support from the DARPA Nimbus program. The data are
available from Gaopeng Lu (gaopenglu@gmail.com).
NR 48
TC 0
Z9 0
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2016
VL 121
IS 8
BP 4082
EP 4092
DI 10.1002/2015JD024644
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP2KU
UT WOS:000378318100020
ER
PT J
AU Miller, DJ
Zhang, ZB
Ackerman, AS
Platnick, S
Baum, BA
AF Miller, Daniel J.
Zhang, Zhibo
Ackerman, Andrew S.
Platnick, Steven
Baum, Bryan A.
TI The impact of cloud vertical profile on liquid water path retrieval
based on the bispectral method: A theoretical study based on large-eddy
simulations of shallow marine boundary layer clouds
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SATELLITE-OBSERVATIONS; RADIATIVE-TRANSFER; OPTICAL-THICKNESS;
STRATIFORM CLOUDS; EFFECTIVE RADIUS; PART I; STRATOCUMULUS; MODIS;
AEROSOL; MICROPHYSICS
AB Passive optical retrievals of cloud liquid water path (LWP), like those implemented for Moderate Resolution Imaging Spectroradiometer (MODIS), rely on cloud vertical profile assumptions to relate optical thickness (tau) and effective radius (r(e)) retrievals to LWP. These techniques typically assume that shallow clouds are vertically homogeneous; however, an adiabatic cloud model is plausibly more realistic for shallow marine boundary layer cloud regimes. In this study a satellite retrieval simulator is used to perform MODIS-like satellite retrievals, which in turn are compared directly to the large-eddy simulation (LES) output. This satellite simulator creates a framework for rigorous quantification of the impact that vertical profile features have on LWP retrievals, and it accomplishes this while also avoiding sources of bias present in previous observational studies. The cloud vertical profiles from the LES are often more complex than either of the two standard assumptions, and the favored assumption was found to be sensitive to cloud regime (cumuliform/stratiform). Confirming previous studies, drizzle and cloud top entrainment of dry air are identified as physical features that bias LWP retrievals away from adiabatic and toward homogeneous assumptions. The mean bias induced by drizzle-influenced profiles was shown to be on the order of 5-10 g/m(2). In contrast, the influence of cloud top entrainment was found to be smaller by about a factor of 2. A theoretical framework is developed to explain variability in LWP retrievals by introducingmodifications to the adiabatic re profile. In addition to analyzing bispectral retrievals, we also compare results with the vertical profile sensitivity of passive polarimetric retrieval techniques.
C1 [Miller, Daniel J.; Zhang, Zhibo] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA.
[Zhang, Zhibo] Joint Ctr Earth Syst Technol, Baltimore, MD USA.
[Ackerman, Andrew S.] NASA Goddard Inst Space Studies, New York, NY USA.
[Platnick, Steven] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Baum, Bryan A.] Univ Wisconsin, Ctr Space Sci & Engn, 1225 W Dayton St, Madison, WI 53706 USA.
RP Miller, DJ (reprint author), Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA.
EM dj-miller@umbc.edu
RI Baum, Bryan/B-7670-2011; Platnick, Steven/J-9982-2014; Zhang,
Zhibo/D-1710-2010
OI Baum, Bryan/0000-0002-7193-2767; Platnick, Steven/0000-0003-3964-3567;
Zhang, Zhibo/0000-0001-9491-1654
FU NASA [NNX11AR06G, NNX14AJ25G]; HalMaring at NASA Headquarters; U.S.
National Science Foundation through the MRI program [CNS-0821258,
CNS-1228778]; SCREMS program [DMS-0821311]; University of Maryland,
Baltimore County (UMBC)
FX This work was funded in part through NASA grants NNX11AR06G and
NNX14AJ25G. The authors appreciate the continuing support of HalMaring
at NASA Headquarters. D.J.M. acknowledges the NASA Earth and Space
Science Fellowship (NESSF) managed by Ming-Ying Wei. The hardware used
in the computational studies is part of the UMBC High Performance
Computing Facility (HPCF). The facility is supported by the U.S.
National Science Foundation through the MRI program (grants CNS-0821258
and CNS-1228778) and the SCREMS program (grant DMS-0821311), with
additional substantial support from the University of Maryland,
Baltimore County (UMBC).
NR 42
TC 1
Z9 1
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2016
VL 121
IS 8
BP 4122
EP 4141
DI 10.1002/2015JD024322
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP2KU
UT WOS:000378318100024
ER
PT J
AU Shingler, T
Crosbie, E
Ortega, A
Shiraiwa, M
Zuend, A
Beyersdorf, A
Ziemba, L
Anderson, B
Thornhill, L
Perring, AE
Schwarz, JP
Campazano-Jost, P
Day, DA
Jimenez, JL
Hair, JW
Mikoviny, T
Wisthaler, A
Sorooshian, A
AF Shingler, Taylor
Crosbie, Ewan
Ortega, Amber
Shiraiwa, Manabu
Zuend, Andreas
Beyersdorf, Andreas
Ziemba, Luke
Anderson, Bruce
Thornhill, Lee
Perring, Anne E.
Schwarz, Joshua P.
Campazano-Jost, Pedro
Day, Douglas A.
Jimenez, Jose L.
Hair, Johnathan W.
Mikoviny, Tomas
Wisthaler, Armin
Sorooshian, Armin
TI Airborne characterization of subsaturated aerosol hygroscopicity and dry
refractive index from the surface to 6.5km during the SEAC(4)RS campaign
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ORGANIC-INORGANIC AEROSOLS; SINGLE-SCATTERING ALBEDO; LIQUID-LIQUID
EQUILIBRIA; OPTICAL-PROPERTIES; AMMONIUM-SULFATE; LIGHT-SCATTERING;
ACTIVITY-COEFFICIENTS; RADIATIVE PROPERTIES; CHEMICAL-COMPOSITION;
THERMODYNAMIC MODEL
AB In situ aerosol particle measurements were conducted during 21 NASA DC-8 flights in the Studies of Emissions and Atmospheric Composition, Clouds, and Climate Coupling by Regional Surveys field campaign over the United States, Canada, Pacific Ocean, and Gulf of Mexico. For the first time, this study reports rapid, size-resolved hygroscopic growth and real refractive index (RI at 532 nm) data between the surface and upper troposphere in a variety of air masses including wildfires, agricultural fires, biogenic, marine, and urban outflow. The Differential Aerosol Sizing and Hygroscopicity Spectrometer Probe (DASH-SP) quantified size-resolved diameter growth factors (GF = D-p,D-wet/D-p,D-dry) that are used to infer the hygroscopicity parameter kappa. Thermokinetic simulations were conducted to estimate the impact of partial particle volatilization within the DASH-SP across a range of sampling conditions. Analyses of GF and RI data as a function of air mass origin, dry size, and altitude are reported, in addition to kappa values for the inorganic and organic fractions of aerosol. Average RI values are found to be fairly constant (1.52-1.54) for all air mass categories. An algorithm is used to compare size-resolved DASH-SP GF with bulk scattering f(RH=80%) data obtained from a pair of nephelometers, and the results show that the two can only be reconciled if GF is assumed to decrease with increasing dry size above 400 nm (i.e., beyond the upper bound of DASH-SP measurements). Individual case studies illustrate variations of hygroscopicity as a function of dry size, environmental conditions, altitude, and composition.
C1 [Shingler, Taylor; Ortega, Amber; Sorooshian, Armin] Univ Arizona, Dept Chem & Environm Engn, Tucson, AZ USA.
[Crosbie, Ewan; Beyersdorf, Andreas; Ziemba, Luke; Anderson, Bruce; Thornhill, Lee; Hair, Johnathan W.] NASA, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23665 USA.
[Crosbie, Ewan] Oak Ridge Associated Univ, Oak Ridge, TN USA.
[Shiraiwa, Manabu] Max Planck Inst Chem, Multiphase Chem Dept, Mainz, Germany.
[Zuend, Andreas] McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ, Canada.
[Thornhill, Lee] Sci Syst & Applicat Inc, Hampton, VA USA.
[Perring, Anne E.; Schwarz, Joshua P.] NOAA, Chem Sci Div, Earth Syst Res Lab, Boulder, CO USA.
[Perring, Anne E.; Campazano-Jost, Pedro; Day, Douglas A.; Jimenez, Jose L.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Campazano-Jost, Pedro; Day, Douglas A.; Jimenez, Jose L.] Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA.
[Mikoviny, Tomas; Wisthaler, Armin] Univ Oslo, Dept Chem, Oslo, Norway.
[Wisthaler, Armin] Univ Innsbruck, Inst Ion Phys & Appl Phys, A-6020 Innsbruck, Austria.
[Sorooshian, Armin] Univ Arizona, Dept Atmospher Sci, Tucson, AZ USA.
RP Sorooshian, A (reprint author), Univ Arizona, Dept Chem & Environm Engn, Tucson, AZ USA.; Sorooshian, A (reprint author), Univ Arizona, Dept Atmospher Sci, Tucson, AZ USA.
EM armin@email.arizona.edu
RI Perring, Anne/G-4597-2013; Jimenez, Jose/A-5294-2008; schwarz,
joshua/G-4556-2013; Manager, CSD Publications/B-2789-2015
OI Perring, Anne/0000-0003-2231-7503; Jimenez, Jose/0000-0001-6203-1847;
schwarz, joshua/0000-0002-9123-2223;
FU NASA [NNX12AC10G, NNX14AP75G, NNX12AC03G, NNX15AT96G]; ONR
[N00014-10-1-0811]; NASA Earth and Space Science Fellowship
[NNX14AK79H]; Visiting Scientist Program at the National Institute of
Aerospace
FX All data and results are available from the corresponding author
(armin@email.arizona.edu). This research was funded by NASA grants
NNX12AC10G and NNX14AP75G. The development of the DASH-SP instrument was
funded by ONR grant N00014-10-1-0811. T.S. acknowledges support from a
NASA Earth and Space Science Fellowship (NNX14AK79H). P.C.J., D.A.D.,
and J.L.J. were supported by NASA grants NNX12AC03G and NNX15AT96G.
PTR-MS measurements during SEAC4RS were supported by the
Austrian Federal Ministry for Transport, Innovation and Technology
(bmvit) through the Austrian Space Applications Programme of the
Austrian Research Promotion Agency (FFG). A.W. and T.M. received support
from the Visiting Scientist Program at the National Institute of
Aerospace.
NR 98
TC 5
Z9 5
U1 8
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2016
VL 121
IS 8
BP 4188
EP 4210
DI 10.1002/2015JD024498
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP2KU
UT WOS:000378318100028
ER
PT J
AU Griffith, SM
Hansen, RF
Dusanter, S
Michoud, V
Gilman, JB
Kuster, WC
Veres, PR
Graus, M
de Gouw, JA
Roberts, J
Young, C
Washenfelder, R
Brown, SS
Thalman, R
Waxman, E
Volkamer, R
Tsai, C
Stutz, J
Flynn, JH
Grossberg, N
Lefer, B
Alvarez, SL
Rappenglueck, B
Mielke, LH
Osthoff, HD
Stevens, PS
AF Griffith, S. M.
Hansen, R. F.
Dusanter, S.
Michoud, V.
Gilman, J. B.
Kuster, W. C.
Veres, P. R.
Graus, M.
de Gouw, J. A.
Roberts, J.
Young, C.
Washenfelder, R.
Brown, S. S.
Thalman, R.
Waxman, E.
Volkamer, R.
Tsai, C.
Stutz, J.
Flynn, J. H.
Grossberg, N.
Lefer, B.
Alvarez, S. L.
Rappenglueck, B.
Mielke, L. H.
Osthoff, H. D.
Stevens, P. S.
TI Measurements of hydroxyl and hydroperoxy radicals during CalNex-LA:
Model comparisons and radical budgets
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LASER-INDUCED FLUORESCENCE; IONIZATION MASS-SPECTROMETRY; VOLATILE
ORGANIC-COMPOUNDS; MCMA-2006 FIELD CAMPAIGN; MEXICO-CITY ATMOSPHERE;
MISSING OH SOURCE; NEW-YORK-CITY; NI-PT-CIMS; HO2 CONCENTRATIONS;
LOS-ANGELES
AB Measurements of hydroxyl (OH) and hydroperoxy (HO2*) radical concentrations were made at the Pasadena ground site during the CalNex-LA 2010 campaign using the laser-induced fluorescence-fluorescence assay by gas expansion technique. The measured concentrations of OH and HO2* exhibited a distinct weekend effect, with higher radical concentrations observed on the weekends corresponding to lower levels of nitrogen oxides (NOx). The radical measurements were compared to results from a zero-dimensional model using the Regional Atmospheric Chemical Mechanism-2 constrained by NOx and othermeasured trace gases. The chemical model overpredicted measured OH concentrations during the weekends by a factor of approximately 1.4 +/- 0.3 (1 sigma), but the agreement was better during the weekdays (ratio of 1.0 +/- 0.2). Model predicted HO2* concentrations underpredicted by a factor of 1.3 +/- 0.2 on the weekends, while measured weekday concentrations were underpredicted by a factor of 3.0 +/- 0.5. However, increasing the modeled OH reactivity to match the measured total OH reactivity improved the overall agreement for both OH and HO2* on all days. A radical budget analysis suggests that photolysis of carbonyls and formaldehyde together accounted for approximately 40% of radical initiation with photolysis of nitrous acid accounting for 30% at the measurement height and ozone photolysis contributing less than 20%. An analysis of the ozone production sensitivity reveals that during the week, ozone production was limited by volatile organic compounds throughout the day during the campaign but NOx limited during the afternoon on the weekends.
C1 [Griffith, S. M.; Dusanter, S.; Stevens, P. S.] Indiana Univ, Sch Publ & Environm Affairs, Bloomington, IN USA.
[Griffith, S. M.] Hong Kong Univ Sci & Technol, Dept Chem, Hong Kong, Hong Kong, Peoples R China.
[Hansen, R. F.; Stevens, P. S.] Indiana Univ, Dept Chem, Bloomington, IN USA.
[Hansen, R. F.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England.
[Dusanter, S.; Michoud, V.] SAGE, Mines Douai, Douai, France.
[Dusanter, S.; Michoud, V.] Univ Lille, Lille, France.
[Michoud, V.] UPEC, Lab Interunivers Syst Atmospher, LISA IPSL, UMR CNRS 7583, Creteil, France.
[Michoud, V.] UPD, Creteil, France.
[Gilman, J. B.; Veres, P. R.; Graus, M.; de Gouw, J. A.; Roberts, J.; Young, C.; Washenfelder, R.; Brown, S. S.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Gilman, J. B.; Kuster, W. C.; Veres, P. R.; Graus, M.; de Gouw, J. A.; Roberts, J.; Young, C.; Washenfelder, R.; Brown, S. S.] NOAA, Chem Sci Div, Earth Syst Res Lab, Boulder, CO USA.
[Graus, M.] Univ Innsbruck, Inst Atmospher & Cryospher Sci, A-6020 Innsbruck, Austria.
[Young, C.] Mem Univ Newfoundland, Dept Chem, St John, NF A1B 3X7, Canada.
[Thalman, R.; Waxman, E.; Volkamer, R.] Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA.
[Thalman, R.; Waxman, E.; Volkamer, R.] Univ Colorado, CIRES, Boulder, CO 80309 USA.
[Thalman, R.] Snow Coll, Dept Chem, Ephraim, UT USA.
[Tsai, C.; Stutz, J.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Flynn, J. H.; Grossberg, N.; Lefer, B.; Alvarez, S. L.; Rappenglueck, B.] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX USA.
[Lefer, B.] NASA Headquarters, Div Earth Sci, Washington, DC USA.
[Mielke, L. H.; Osthoff, H. D.] Univ Calgary, Dept Chem, Calgary, AB T2N 1N4, Canada.
[Mielke, L. H.] Univ Indianapolis, Dept Chem, Indianapolis, IN 46227 USA.
RP Stevens, PS (reprint author), Indiana Univ, Sch Publ & Environm Affairs, Bloomington, IN USA.; Stevens, PS (reprint author), Indiana Univ, Dept Chem, Bloomington, IN USA.
EM pstevens@indiana.edu
RI de Gouw, Joost/A-9675-2008; Veres, Patrick/E-7441-2010; Young,
Cora/A-4551-2010; Lefer, Barry/B-5417-2012; Manager, CSD
Publications/B-2789-2015; Volkamer, Rainer/B-8925-2016; Gilman,
Jessica/E-7751-2010; Brown, Steven/I-1762-2013; Graus,
Martin/E-7546-2010; Roberts, James/A-1082-2009; Washenfelder,
Rebecca/E-7169-2010
OI de Gouw, Joost/0000-0002-0385-1826; Veres, Patrick/0000-0001-7539-353X;
Young, Cora/0000-0002-6908-5829; Lefer, Barry/0000-0001-9520-5495;
Osthoff, Hans/0000-0001-7155-6493; Volkamer, Rainer/0000-0002-0899-1369;
Gilman, Jessica/0000-0002-7899-9948; Graus, Martin/0000-0002-2025-9242;
Roberts, James/0000-0002-8485-8172; Washenfelder,
Rebecca/0000-0002-8106-3702
FU National Science Foundation [AGS-0612738, AGS-1104880]
FX This work was supported by grants from the National Science Foundation
(AGS-0612738 and AGS-1104880). We would also like to thank the
California Air Resources Board and the California Institute of
Technology for their support of the CalNex-LA ground site. We would also
like to thank Jean Francois Doussin and Marie Camredon from LISA for
their valuable discussion. Data presented in this manuscript can be
requested by contacting the corresponding author and can also be found
at http://www.esrl.noaa.gov/csd/projects/calnex/.
NR 83
TC 4
Z9 4
U1 23
U2 33
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2016
VL 121
IS 8
BP 4211
EP 4232
DI 10.1002/2015JD024358
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP2KU
UT WOS:000378318100029
ER
PT J
AU Bela, MM
Barth, MC
Toon, OB
Fried, A
Homeyer, CR
Morrison, H
Cummings, KA
Li, YY
Pickering, KE
Allen, DJ
Yang, Q
Wennberg, PO
Crounse, JD
St Clair, JM
Teng, AP
O'Sullivan, D
Huey, LG
Chen, DX
Liu, XX
Blake, DR
Blake, NJ
Apel, EC
Hornbrook, RS
Flocke, F
Campos, T
Diskin, G
AF Bela, Megan M.
Barth, Mary C.
Toon, Owen B.
Fried, Alan
Homeyer, Cameron R.
Morrison, Hugh
Cummings, Kristin A.
Li, Yunyao
Pickering, Kenneth E.
Allen, Dale J.
Yang, Qing
Wennberg, Paul O.
Crounse, John D.
St Clair, Jason M.
Teng, Alex P.
O'Sullivan, Daniel
Huey, L. Gregory
Chen, Dexian
Liu, Xiaoxi
Blake, Donald R.
Blake, Nicola J.
Apel, Eric C.
Hornbrook, Rebecca S.
Flocke, Frank
Campos, Teresa
Diskin, Glenn
TI Wet scavenging of soluble gases in DC3 deep convective storms using
WRF-Chem simulations and aircraft observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID IONIZATION MASS-SPECTROMETRY; UPPER TROPOSPHERE; HYDROGEN-PEROXIDE;
TRACE GASES; RADAR OBSERVATIONS; MODEL PERFORMANCE; MOIST CONVECTION;
CENTRAL VIRGINIA; HIGH-SENSITIVITY; SULFUR-DIOXIDE
AB We examine wet scavenging of soluble trace gases in storms observed during the Deep Convective Clouds and Chemistry (DC3) field campaign. We conduct high-resolution simulations with the Weather Research and Forecasting model with Chemistry (WRF-Chem) of a severe storm in Oklahoma. The model represents well the storm location, size, and structure as compared with Next Generation Weather Radar reflectivity, and simulated CO transport is consistent with aircraft observations. Scavenging efficiencies (SEs) between inflow and outflow of soluble species are calculated from aircraft measurements and model simulations. Using a simple wet scavenging scheme, we simulate the SE of each soluble species within the error bars of the observations. The simulated SEs of all species except nitric acid (HNO3) are highly sensitive to the values specified for the fractions retained in ice when cloud water freezes. To reproduce the observations, we must assume zero ice retention for formaldehyde (CH2O) and hydrogen peroxide (H2O2) and complete retention for methyl hydrogen peroxide (CH3OOH) and sulfur dioxide (SO2), likely to compensate for the lack of aqueous chemistry in the model. We then compare scavenging efficiencies among storms that formed in Alabama and northeast Colorado and the Oklahoma storm. Significant differences in SEs are seen among storms and species. More scavenging of HNO3 and less removal of CH3OOH are seen in storms with higher maximum flash rates, an indication of more graupel mass. Graupel is associated with mixed-phase scavenging and lightning production of nitrogen oxides (NOx), processes that may explain the observed differences in HNO3 and CH3OOH scavenging.
C1 [Bela, Megan M.; Toon, Owen B.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Bela, Megan M.; Toon, Owen B.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Barth, Mary C.; Morrison, Hugh; Apel, Eric C.; Hornbrook, Rebecca S.; Flocke, Frank; Campos, Teresa] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Fried, Alan] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Homeyer, Cameron R.] Univ Oklahoma, Sch Meteorol, Norman, OK 73019 USA.
[Cummings, Kristin A.; Li, Yunyao; Pickering, Kenneth E.; Allen, Dale J.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Pickering, Kenneth E.; St Clair, Jason M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Yang, Qing] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Wennberg, Paul O.; Crounse, John D.; St Clair, Jason M.; Teng, Alex P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Wennberg, Paul O.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
[St Clair, Jason M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[O'Sullivan, Daniel] US Naval Acad, Annapolis, MD 21402 USA.
[Huey, L. Gregory; Chen, Dexian; Liu, Xiaoxi] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Blake, Donald R.; Blake, Nicola J.] Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA.
[Diskin, Glenn] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Bela, MM (reprint author), Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.; Bela, MM (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
EM megan.bela@colorado.edu
RI Pickering, Kenneth/E-6274-2012; Homeyer, Cameron/D-5034-2013; Allen,
Dale/F-7168-2010; Crounse, John/C-3700-2014
OI Homeyer, Cameron/0000-0002-4883-6670; Allen, Dale/0000-0003-3305-9669;
Crounse, John/0000-0001-5443-729X
FU National Science Foundation; NSF [AGS-1261559, AGS-1522910, 1063479,
1522551, ATM1063467]; NASA [ACCDAMNNX14AR56G, NNX12AMO8G, NNX12AC06G,
NNX14AP46G-ACCDAM, NNX12AB77G, NNX12AB76G]; Office of Science of the
U.S. Department of Energy as part of the Atmospheric System Research
Program (ASR)
FX We express our appreciation to the following researchers for the
aircraft observations: T. Ryerson and the NOAA
NOyO3 team; Andrew Weinheimer; Mark Zondlo, Josh
DiGangi, and Anthony O'Brien for the VCSEL hygrometer water vapor
measurements on the GV; and P. Lawson and S. Woods from SPEC Inc. We
also thank A. Weinheimer and M. Zondlo for their helpful feedback on
this manuscript. M. M. Bela and O.B. Toon were supported by NASA
ACCDAMNNX14AR56G. The National Center for Atmospheric Research is
sponsored by the National Science Foundation. A. Fried was supported by
NSF and NASA under grants AGS-1261559 and NNX12AMO8G, respectively. C.
Homeyer was funded by NSF grant AGS-1522910. The University of Maryland
co-authors were supported under NSF grants 1063479 and 1522551. Q. Yang
was supported by the Office of Science of the U.S. Department of Energy
as part of the Atmospheric System Research Program (ASR). P.O. Wennberg,
J.D. Crounse, A. P. Teng, and J.M. St. Clair thank NASA for supporting
their contribution to this study (NNX12AC06G and NNX14AP46G-ACCDAM). D.
O'Sullivan thanks NSF for support from grant ATM1063467. L.G. Huey, D.
Chen, and X. Liu were funded by NASA grant NNX12AB77G. DC3 measurements
by N. Blake and D. Blake were supported by NASA award NNX12AB76G. We
would like to thank Earth Networks for providing the ENTLN lightning
data for research purposes. The data used in this study can be
downloaded from the following websites: 1 s data merges from the NASA
Langley DC3 Merged Aircraft Dataset Archive
(http://www-air.larc.nasa.gov/cgi-bin/ArcView/dc3); NEXRAD data for
individual radars from the National Climatic Data Center (NCDC;
http://has.ncdc.noaa.gov/pls/plhas/has.dsselect); NSSL-MGAUS sounding
data (http://data.eol.ucar.edu/codiac/dss/id=353.105); NCEP Stage IV
precipitation analysis
(http://www.emc.ncep.noaa.gov/mmb/ylin/pcpanl/stage4/); and NAM-ANL
(http://nomads.ncdc.noaa.gov/data/namanl/). The WRF-Chem code and land
surface data are available for download from NCAR/MMM
(http://www.mmm.ucar.edu/wrf/users/download/get_sources_wps_geog.html).
WRF-Chem model output is available upon request to M. M. Bela
(megan.bela@colorado.edu).
NR 104
TC 4
Z9 4
U1 4
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2016
VL 121
IS 8
BP 4233
EP 4257
DI 10.1002/2015JD024623
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP2KU
UT WOS:000378318100030
ER
PT J
AU Barth, MC
Bela, MM
Fried, A
Wennberg, PO
Crounse, JD
St Clair, JM
Blake, NJ
Blake, DR
Homeyer, CR
Brune, WH
Zhang, L
Mao, J
Ren, X
Ryerson, TB
Pollack, IB
Peischl, J
Cohen, RC
Nault, BA
Huey, LG
Liu, X
Cantrell, CA
AF Barth, M. C.
Bela, M. M.
Fried, A.
Wennberg, P. O.
Crounse, J. D.
St Clair, J. M.
Blake, N. J.
Blake, D. R.
Homeyer, C. R.
Brune, W. H.
Zhang, L.
Mao, J.
Ren, X.
Ryerson, T. B.
Pollack, I. B.
Peischl, J.
Cohen, R. C.
Nault, B. A.
Huey, L. G.
Liu, X.
Cantrell, C. A.
TI Convective transport and scavenging of peroxides by thunderstorms
observed over the central US during DC3
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID VOLATILE ORGANIC-COMPOUNDS; STRATOSPHERIC-TROPOSPHERIC EXPERIMENT;
TROPICAL UPPER TROPOSPHERE; GAS-PHASE; NUMERICAL SIMULATIONS; RADAR
OBSERVATIONS; HYDROGEN-PEROXIDE; UNITED-STATES; TRACE GASES; JULY 10
AB One of the objectives of the Deep Convective Clouds and Chemistry (DC3) field experiment was to determine the scavenging of soluble trace gases by thunderstorms. We present an analysis of scavenging of hydrogen peroxide (H2O2) and methyl hydrogen peroxide (CH3OOH) from six DC3 cases that occurred in Oklahoma and northeast Colorado. Estimates of H2O2 scavenging efficiencies are comparable to previous studies ranging from 79 to 97% with relative uncertainties of 5-25%. CH3OOH scavenging efficiencies ranged from 12 to 84% with relative uncertainties of 18-558%. The wide range of CH3OOH scavenging efficiencies is surprising, as previous studies suggested that CH3OOH scavenging efficiencies would be < 10%. Cloud chemistry model simulations of one DC3 storm produced CH3OOH scavenging efficiencies of 26-61% depending on the ice retention factor of CH3OOH during cloud drop freezing, suggesting ice physics impacts CH3OOH scavenging. The highest CH3OOH scavenging efficiencies occurred in two severe thunderstorms, but there is no obvious correlation between the CH3OOH scavenging efficiency and the storm thermodynamic environment. We found a moderate correlation between the estimated entrainment rates and CH3OOH scavenging efficiencies. Changes in gas-phase chemistry due to lightning production of nitric oxide and aqueous-phase chemistry have little effect on CH3OOH scavenging efficiencies. To determine why CH3OOH can be substantially removed from storms, future studies should examine effects of entrainment rate, retention of CH3OOH in frozen cloud particles during drop freezing, and lightning-NOx production.
C1 [Barth, M. C.] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
[Barth, M. C.] Natl Ctr Atmospher Res, Mesoscale & Microscale Meteorol Lab, POB 3000, Boulder, CO 80307 USA.
[Bela, M. M.; Cantrell, C. A.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Bela, M. M.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Fried, A.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Wennberg, P. O.; Crounse, J. D.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[St Clair, J. M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Blake, N. J.; Blake, D. R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA.
[Homeyer, C. R.] Univ Oklahoma, Sch Meteorol, Norman, OK 73019 USA.
[Brune, W. H.; Zhang, L.] Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA.
[Mao, J.] Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA.
[Mao, J.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Ren, X.] NOAA Air Resources Lab, College Pk, MD USA.
[Ryerson, T. B.; Peischl, J.] NOAA, Chem Sci Div, Earth Syst Res Lab, Boulder, CO USA.
[Pollack, I. B.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Peischl, J.; Nault, B. A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Cohen, R. C.; Nault, B. A.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Nault, B. A.] Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA.
[Huey, L. G.; Liu, X.] Georgia Inst Technol, Atlanta, GA 30332 USA.
RP Barth, MC (reprint author), Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.; Barth, MC (reprint author), Natl Ctr Atmospher Res, Mesoscale & Microscale Meteorol Lab, POB 3000, Boulder, CO 80307 USA.
EM barthm@ucar.edu
RI Peischl, Jeff/E-7454-2010; Cohen, Ronald/A-8842-2011; Ren,
Xinrong/E-7838-2015; Pollack, Ilana/F-9875-2012; Mao,
Jingqiu/F-2511-2010; Homeyer, Cameron/D-5034-2013; Crounse,
John/C-3700-2014; Manager, CSD Publications/B-2789-2015
OI Peischl, Jeff/0000-0002-9320-7101; Cohen, Ronald/0000-0001-6617-7691;
Ren, Xinrong/0000-0001-9974-1666; Mao, Jingqiu/0000-0002-4774-9751;
Homeyer, Cameron/0000-0002-4883-6670; Crounse, John/0000-0001-5443-729X;
FU National Science Foundation; NSF [AGS-1261559, AGS-1522910, DGE
1106400]; NASA [NNX12AMO8G, NNX12AC06G, NNX14AP46G-ACCDAM, NNX12AB76G,
NNX12AB84G, NNX12AB79G, NNX12AB77G]; NOAA Climate Change program by NASA
[NNH12AT30I]; NOAA Health of the Atmosphere program [NNH12AT30I]
FX The authors thank the DC3 Science and Logistics teams for the successful
execution of the DC3 field campaign. Data from the DC3 field project can
be found at http://data.eol.ucar.edu/master_list/?project=DC3. The
aircraft data are also located at
http://www-air.larc.nasa.gov/cgi-bin/ArcView/dc3-seac4rs. Output from
the model simulations can be obtained upon request to M. Barth
(barthm@ucar.edu). We appreciate Conrad Ziegler (NOAA/NSSL) and his team
as well as the NCAR/EOL ISS team for the radiosonde data. G. Diskin and
his team are acknowledged for their DC-8 water vapor and CO
measurements. We are grateful for the informative weather summaries
provided by Morris Weisman and Craig Schwartz during the DC3 field
campaign. We value the contributions of John Orlando and the comments on
the paper by Sasha Madronich, Rebecca Hornbrook and the three anonymous
reviewers. The National Center for Atmospheric Research is sponsored by
the National Science Foundation. The INSTAAR group acknowledges NSF and
NASA under grant awards AGS-1261559 and NNX12AMO8G, respectively, for
funding their participation in the measurements and analysis. The
Caltech group thanks NASA for funding their participation in DC3 and
contribution to this analysis via grants NNX12AC06G and
NNX14AP46G-ACCDAM. N. Blake and D. Blake acknowledge support for DC3
measurements from NASA award NNX12AB76G. C. Homeyer was supported by NSF
under grant AGS-1522910. W. H. Brune, L. Zhang, J. Mao, and X. Ren were
supported by NASA grant NNX12AB84G. T. B. Ryerson, J. Peischl, and I. B.
Pollack were supported under the NOAA Climate Change and NOAA Health of
the Atmosphere programs, with participation in DC3 made possible by NASA
grant NNH12AT30I. R. C. Cohen and B. A. Nault were supported by NASA
grant NNX12AB79G. B. A. Nault was also supported by the NSF Graduate
Research Fellowship under grant DGE 1106400. L. G. Huey and X. Liu were
supported by NASA grant NNX12AB77G.
NR 70
TC 3
Z9 3
U1 5
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2016
VL 121
IS 8
BP 4272
EP 4295
DI 10.1002/2015JD024570
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP2KU
UT WOS:000378318100032
ER
PT J
AU Field, RD
Luo, M
Fromm, M
Voulgarakis, A
Mangeon, S
Worden, J
AF Field, Robert D.
Luo, Ming
Fromm, Mike
Voulgarakis, Apostolos
Mangeon, Stephane
Worden, John
TI Simulating the Black Saturday 2009 smoke plume with an interactive
composition-climate model: Sensitivity to emissions amount, timing, and
injection height
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID BIOMASS BURNING EMISSIONS; TRANSFORM INFRARED-SPECTROSCOPY; AUSTRALIAN
VEGETATION FIRES; INTERANNUAL VARIABILITY; ACCURATE SIMULATION;
CHEMICAL-MODELS; TRACE GASES; AEROSOLS; IMPACT; FUTURE
AB We simulated the high-altitude smoke plume from the early February 2009 Black Saturday bushfires in southeastern Australia using the NASA Goddard Institute for Space Studies ModelE2. To the best of our knowledge, this is the first single-plume analysis of biomass burning emissions injected directly into the upper troposphere/lower stratosphere (UTLS) using a full-complexity composition-climate model. We compared simulated carbon monoxide (CO) to a new Aura Tropospheric Emission Spectrometer/Microwave Limb Sounder joint CO retrieval, focusing on the plume's initial transport eastward, anticyclonic circulation to the north of New Zealand, westward transport in the lower stratospheric easterlies, and arrival over Africa at the end of February. Our goal was to determine the sensitivity of the simulated plume to prescribed injection height, emissions amount, and emissions timing from different sources for a full-complexity model when compared to Aura. The most realistic plumes were obtained using injection heights in the UTLS, including one drawn from ground-based radar data. A 6 h emissions pulse or emissions tied to independent estimates of hourly fire behavior produced a more realistic plume in the lower stratosphere compared to the same emissions amount being released evenly over 12 or 24 h. Simulated CO in the plume was highly sensitive to the differences between emissions amounts estimated from the Global Fire Emissions Database and from detailed, ground-based estimates of fire growth. The emissions amount determined not only the CO concentration of the plume but also the proportion of the plume that entered the stratosphere. We speculate that this is due to either or both nonlinear CO loss with a weakened OH sink or plume self-lofting driven by shortwave absorption of the coemitted aerosols.
C1 [Field, Robert D.] NASA Goddard Inst Space Studies, New York, NY USA.
[Field, Robert D.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Luo, Ming; Worden, John] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Fromm, Mike] Naval Res Lab, Washington, DC 20375 USA.
[Voulgarakis, Apostolos; Mangeon, Stephane] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London, England.
RP Field, RD (reprint author), NASA Goddard Inst Space Studies, New York, NY USA.; Field, RD (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
EM robert.field@columbia.edu
FU NASA ROSES Atmospheric Modeling and Analysis Program [NNX13AK46G];
Natural Environment Research Council; UK Met Office; NASA High-End
Computing (HEC) Program through the NASA Center for Climate Simulation
(NCCS) at Goddard Space Flight Center; Jet Propulsion Laboratory,
California Institute of Technology
FX Laverton and Yarrowonga Radar data were obtained from the Australian
Bureau of Meteorology. We thank Nicholas Gellie for the use of his
unpublished area burned estimates for the Black Saturday fires. R.D.F.
and M.F. were supported by NASA ROSES Atmospheric Modeling and Analysis
Program grant NNX13AK46G. A.V. and S.M. were supported by the Natural
Environment Research Council and the UK Met Office. Research was
partially supported by the Jet Propulsion Laboratory, California
Institute of Technology under contract to the National Aeronautics and
Space Administration (NASA). Resources supporting this work were
provided by the NASA High-End Computing (HEC) Program through the NASA
Center for Climate Simulation (NCCS) at Goddard Space Flight Center. All
data in the study can be obtained by contacting the lead author.
NR 61
TC 0
Z9 0
U1 5
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2016
VL 121
IS 8
BP 4296
EP 4316
DI 10.1002/2015JD024343
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP2KU
UT WOS:000378318100033
ER
PT J
AU Meyyappan, M
AF Meyyappan, M.
TI Carbon Nanotube-Based Chemical Sensors
SO SMALL
LA English
DT Review
DE chemical sensors; carbon nanotubes; chemiresistors; electronic noses;
gas sensing; vapor sensing
ID GAS-SENSING PROPERTIES; ROOM-TEMPERATURE; VAPOR DETECTION; NO2 GAS;
CHEMIRESISTIVE SENSORS; SELECTIVE DETECTION; AMMONIA SENSORS; ELECTRONIC
NOSE; SENSITIVITY; ARRAY
AB The need to sense gases and vapors arises in numerous scenarios in industrial, environmental, security and medical applications. Traditionally, this activity has utilized bulky instruments to obtain both qualitative and quantitative information on the constituents of the gas mixture. It is ideal to use sensors for this purpose since they are smaller in size and less expensive; however, their performance in the field must match that of established analytical instruments in order to gain acceptance. In this regard, nanomaterials as sensing media offer advantages in sensitivity, preparation of chip-based sensors and construction of electronic nose for selective detection of analytes of interest. This article provides a review of the use of carbon nanotubes in gas and vapor sensing.
C1 [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Meyyappan, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM m.meyyappan@nasa.gov
NR 141
TC 6
Z9 6
U1 67
U2 116
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA POSTFACH 101161, 69451 WEINHEIM, GERMANY
SN 1613-6810
EI 1613-6829
J9 SMALL
JI Small
PD APR 27
PY 2016
VL 12
IS 16
SI SI
BP 2118
EP 2129
DI 10.1002/smll.201502555
PG 12
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied;
Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA DK1YX
UT WOS:000374712700003
PM 26959284
ER
PT J
AU Knox, JC
Ebner, AD
LeVan, MD
Coker, RF
Ritter, JA
AF Knox, James C.
Ebner, Armin D.
LeVan, M. Douglas
Coker, Robert F.
Ritter, James A.
TI Limitations of Breakthrough Curve Analysis in Fixed-Bed Adsorption
SO INDUSTRIAL & ENGINEERING CHEMISTRY RESEARCH
LA English
DT Article
ID PACKED-BEDS; SWING ADSORPTION; AXIAL DIFFUSION; DISPERSION; FLOW; AIR
AB This work examined in detail the a priori prediction of the axial dispersion coefficient from available correlations versus obtaining both it and mass transfer information from experimental breakthrough data and the consequences that may arise when doing so based on using a 1-D axially dispersed plug flow model and its associated Danckwerts outlet boundary condition. These consequences mainly included determining the potential for erroneous extraction of the axial dispersion coefficient and/or the LDF mass transfer coefficient from experimental data, especially when nonplug flow conditions prevailed in the bed. Two adsorbent/adsorbate cases were considered, i.e., CO2 and H2O vapor in zeolite 5A, because they both experimentally exhibited significant nonplug flow behavior, and the H2O-zeolite 5A system exhibited unusual concentration front sharpening that destroyed the expected constant pattern behavior (CPB) when modeled with the 1-D axially dispersed plug flow model. Overall, this work showed that it was possible to extract accurate mass transfer and dispersion information from experimental breakthrough curves using a 1-D axial dispersed plug flow model when they were measured both inside and outside the bed. To ensure the extracted information was accurate, the inside the bed breakthrough curves and their derivatives from the model were plotted to confirm whether or not the adsorbate/adsorbent system was exhibiting CPB or any concentration front sharpening near the bed exit. Even when concentration front sharpening was occurring with the H2O-zeolite 5A system, it was still possible to use the experimental inside and outside the bed breakthrough curves to extract fundamental mass transfer and dispersion information from the 1-D axial dispersed plug flow model based on the systematic methodology developed in this work.
C1 [Knox, James C.; Coker, Robert F.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Ebner, Armin D.; Ritter, James A.] Univ S Carolina, Dept Chem Engn, Columbia, SC 29208 USA.
[LeVan, M. Douglas] Vanderbilt Univ, Dept Chem & Biomol Engn, 221 Kirkland Hall, Nashville, TN 37235 USA.
RP Knox, JC (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM jim.knox@nasa.gov
NR 40
TC 0
Z9 0
U1 8
U2 21
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0888-5885
J9 IND ENG CHEM RES
JI Ind. Eng. Chem. Res.
PD APR 27
PY 2016
VL 55
IS 16
BP 4734
EP 4748
DI 10.1021/acs.iecr.6b00516
PG 15
WC Engineering, Chemical
SC Engineering
GA DK9IU
UT WOS:000375244900036
ER
PT J
AU Ellis, JA
Cornish, NJ
AF Ellis, J. A.
Cornish, N. J.
TI Transdimensional Bayesian approach to pulsar timing noise analysis
SO PHYSICAL REVIEW D
LA English
DT Article
ID BLACK-HOLE BINARIES; MILLISECOND PULSARS; GRAVITATIONAL-WAVES;
DISPERSION; LIMITS
AB The modeling of intrinsic noise in pulsar timing residual data is of crucial importance for gravitational wave detection and pulsar timing (astro)physics in general. The noise budget in pulsars is a collection of several well-studied effects including radiometer noise, pulse-phase jitter noise, dispersion measure variations, and low-frequency spin noise. However, as pulsar timing data continue to improve, nonstationary and non-power-law noise terms are beginning to manifest which are not well modeled by current noise analysis techniques. In this work, we use a transdimensional approach to model these nonstationary and non-power-law effects through the use of a wavelet basis and an interpolation-based adaptive spectral modeling. In both cases, the number of wavelets and the number of control points in the interpolated spectrum are free parameters that are constrained by the data and then marginalized over in the final inferences, thus fully incorporating our ignorance of the noise model. We show that these new methods outperform standard techniques when nonstationary and non-power-law noise is present. We also show that these methods return results consistent with the standard analyses when no such signals are present.
C1 [Ellis, J. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Cornish, N. J.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
RP Ellis, JA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Justin.A.Ellis@jpl.nasa.gov
FU NASA through Einstein Fellowship [PF4-150120]; NSF Physics Frontiers
Center Award [PFC-1430284]; National Science Foundation [PHYS-1066293]
FX J. A. E. acknowledges support by NASA through Einstein Fellowship Grant
No. PF4-150120. N. J. C. was supported by NSF Physics Frontiers Center
Award No. PFC-1430284. Portions of this research were carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. This
work was supported in part by National Science Foundation Grant No.
PHYS-1066293 and by the hospitality of the Aspen Center for Physics,
where this work was initiated.
NR 27
TC 1
Z9 1
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD APR 27
PY 2016
VL 93
IS 8
AR 084048
DI 10.1103/PhysRevD.93.084048
PG 12
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DK5LB
UT WOS:000374960300003
ER
PT J
AU Meng, X
Mannucci, AJ
Verkhoglyadova, OP
Tsurutani, BT
AF Meng, Xing
Mannucci, Anthony J.
Verkhoglyadova, Olga P.
Tsurutani, Bruce T.
TI On forecasting ionospheric total electron content responses to
high-speed solar wind streams
SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE
LA English
DT Article
DE Ionosphere (general); Total electron content (TEC); Modelling;
Forecasting; Storm
ID ELECTRODYNAMIC MODELS; STORMS
AB Conditions in the ionosphere have become increasingly important to forecast, since more and more spaceborne and ground-based technological systems rely on ionospheric weather. Here we explore the feasibility of ionospheric forecasts with the current generation of physics-based models. In particular, we focus on total electron content (TEC) predictions using the Global Ionosphere-Thermosphere Model (GITM). Simulations are configured in a forecast mode and performed for four typical high-speed-stream events during 2007-2012. The simulated TECs are quantified through a metric, which divides the globe into a number of local regions and robustly differentiates between quiet and disturbed periods. Proposed forecast products are hourly global maps color-coded by the TEC disturbance level of each local region. To assess the forecasts, we compare the simulated TEC disturbances with global TEC maps derived from Global Positioning System (GPS) satellite observations. The forecast performance is found to be merely acceptable, with a large number of regions where the observed variations are not captured by the simulations. Examples of model-data agreements and disagreements are investigated in detail, aiming to understand the model behavior and improve future forecasts. For one event, we identify two adjacent regions with similar TEC observations but significant differences in how local chemistry versus plasma transport contribute to electron density changes in the simulation. Suggestions for further analysis are described.
C1 [Meng, Xing; Mannucci, Anthony J.; Verkhoglyadova, Olga P.; Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Meng, X (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM xing.meng@jpl.nasa.gov
NR 31
TC 1
Z9 1
U1 2
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 2115-7251
J9 J SPACE WEATHER SPAC
JI J. Space Weather Space Clim.
PD APR 26
PY 2016
VL 6
AR A19
DI 10.1051/swsc/2016014
PG 11
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA DK5CI
UT WOS:000374936900001
ER
PT J
AU Verkhoglyadova, O
Meng, X
Mannucci, AJ
Tsurutani, BT
Hunt, LA
Mlynczak, MG
Hajra, R
Emery, BA
AF Verkhoglyadova, Olga
Meng, Xing
Mannucci, Anthony J.
Tsurutani, Bruce T.
Hunt, Linda A.
Mlynczak, Martin G.
Hajra, Rajkumar
Emery, Barbara A.
TI Estimation of energy budget of ionosphere-thermosphere system during two
CIR-HSS events: observations and modeling
SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE
LA English
DT Article
DE Ionosphere (general); Thermosphere; Energy distribution; Solar wind;
Modelling
ID FIELD-ALIGNED CURRENT; SPEED SOLAR-WIND; GEOMAGNETIC INDEXES; LESS-THAN;
STORMS; ATMOSPHERE; FLUX; PRECIPITATION; APRIL; DST
AB We analyze the energy budget of the ionosphere-thermosphere (IT) system during two High-Speed Streams (HSSs) on 22-31 January, 2007 (in the descending phase of solar cycle 23) and 25 April-2 May, 2011 (in the ascending phase of solar cycle 24) to understand typical features, similarities, and differences in magnetosphere-ionosphere-thermosphere (IT) coupling during HSS geomagnetic activity. We focus on the solar wind energy input into the magnetosphere (by using coupling functions) and energy partitioning within the IT system during these intervals. The Joule heating is estimated empirically. Hemispheric power is estimated based on satellite measurements. We utilize observations from TIMED/SABER (Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics/Sounding of the Atmosphere using Broadband Emission Radiometry) to estimate nitric oxide (NO) and carbon dioxide (CO2) cooling emission fluxes. We perform a detailed modeling study of these two similar HSS events with the Global Ionosphere-Thermosphere Model (GITM) and different external driving inputs to understand the IT response and to address how well the model reproduces the energy transport. GITM is run in a mode with forecastable inputs. It is shown that the model captures the main features of the energy coupling, but underestimates NO cooling and auroral heating in high latitudes. Lower thermospheric forcing at 100 km altitude is important for correct energy balance of the IT system. We discuss challenges for a physics-based general forecasting approach in modeling the energy budget of moderate IT storms caused by HSSs.
C1 [Verkhoglyadova, Olga; Meng, Xing; Mannucci, Anthony J.; Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Hunt, Linda A.] Sci Syst & Applicat Inc, Hampton, VA 23681 USA.
[Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Hajra, Rajkumar] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Paulo, Brazil.
[Emery, Barbara A.] HAO NCAR, Boulder, CO 80301 USA.
RP Verkhoglyadova, O (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Olga.Verkhoglyadova@jpl.nasa.gov
FU Heliophysics Division of the NASA Science Mission Directorate; NASA
TIMED project office; Brazilian FAPESP agency; National Science
Foundation
FX Portions of this work were done at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA.
Sponsorship of the Heliophysics Division of the NASA Science Mission
Directorate is gratefully acknowledged. MGM would like to acknowledge
support from the NASA TIMED project office. RH would like to thank
Brazilian FAPESP agency for financial support. The computing resources
were provided by the NASA High-End Computing Program through the NASA
Advanced Supercomputing Division at Ames Research Center. SABER data are
available at http://saber.gats-inc.com/. Solar wind parameters and
activity indices are taken from the OMNI database
(http://omniweb.gsfc.nasa.gov/form/omni_min.html). This study used
indices from the CEDAR Database at the National Center for Atmospheric
Research which is supported by the National Science Foundation. The
instant run facility of CCMC was used for the Weimer05 model runs. Solar
radiance was taken from the Space Physics Interactive Data Resource
(http://spidr.ngdc.noaa.gov/spidr/home.do). Flare Irradiance Spectral
Model (FISM) provided empirical solar irradiance spectra
(http://lasp.colorado.edu/lisird/fism/). The ground magnetometer data
was downloaded from the SuperMAG website: http://supermag.jhuapl.edu/).
X. Meng would like to thank A. Ridley (University of Michigan) and Y.
Deng (University of Texas at Arlington, TX) for consulting on the GITM.
OV would like to thank D. Knipp (University of Colorado, Boulder) and Ja
Soon Shim (NASA GSFC) for Poynting flux data samples. The editor thanks
two anonymous referees for their assistance in evaluating this paper.
NR 79
TC 1
Z9 1
U1 1
U2 5
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 2115-7251
J9 J SPACE WEATHER SPAC
JI J. Space Weather Space Clim.
PD APR 26
PY 2016
VL 6
AR A20
DI 10.1051/swsc/2016013
PG 22
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA DK5CI
UT WOS:000374936900002
ER
PT J
AU Gange, G
Navas, JA
Schachte, P
Sondergaard, H
Stuckey, PJ
AF Gange, Graeme
Navas, Jorge A.
Schachte, Peter
Sondergaard, Harald
Stuckey, Peter J.
TI A complete refinement procedure for regular separability of context-free
languages
SO THEORETICAL COMPUTER SCIENCE
LA English
DT Article
DE Abstraction refinement; Context-free languages; Regular approximation;
Separability
ID FREE GRAMMARS
AB Often, when analyzing the behaviour of systems modelled as context-free languages, we wish to know if two languages overlap. To this end, we present a class of semi-decision procedures for regular separability of context-free languages, based on counter-example guided abstraction refinement. We propose two effective instances of this approach, one that is complete but relatively expensive, and one that is inexpensive and sound, but for which we do not have a completeness proof. The complete method will prove disjointness whenever the input languages are regularly separable. Both methods will terminate whenever the input languages overlap. We provide an experimental evaluation of these procedures, and demonstrate their practicality on a range of verification and language-theoretic instances. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Gange, Graeme; Schachte, Peter; Sondergaard, Harald; Stuckey, Peter J.] Univ Melbourne, Dept Comp & Informat Syst, Melbourne, Vic 3010, Australia.
[Navas, Jorge A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Sondergaard, H (reprint author), Univ Melbourne, Dept Comp & Informat Syst, Melbourne, Vic 3010, Australia.
EM gkgange@unimelb.edu.au; jorge.a.navaslaserna@nasa.gov;
schachte@unimelb.edu.au; harald@unimelb.edu.au; pstuckey@unimelb.edu.au
OI Gange, Graeme/0000-0002-1354-431X; Schachte, Peter/0000-0001-5959-3769;
Sondergaard, Harald/0000-0002-2352-1883
FU Australian Research Council [LP140100437]
FX We wish to thank Pierre Ganty for fruitful discussions, and the
anonymous reviewers for their detailed and very constructive feedback;
the paper has been greatly improved as a result of these interactions.
We also wish to thank Georgel Calin for providing the test programs and
the implementation of LCEGAR. Finally we acknowledge support of the
Australian Research Council through Linkage Project grant LP140100437.
NR 27
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0304-3975
EI 1879-2294
J9 THEOR COMPUT SCI
JI Theor. Comput. Sci.
PD APR 25
PY 2016
VL 625
BP 1
EP 24
DI 10.1016/j.tcs.2016.01.026
PG 24
WC Computer Science, Theory & Methods
SC Computer Science
GA DK1YM
UT WOS:000374711600001
ER
PT J
AU Sarikurt, S
Ozden, A
Kandemir, A
Sevik, C
Kinaci, A
Haskins, JB
Cagin, T
AF Sarikurt, S.
Ozden, A.
Kandemir, A.
Sevik, C.
Kinaci, A.
Haskins, J. B.
Cagin, T.
TI Tailoring thermal conductivity of silicon/germanium nanowires utilizing
core-shell architecture
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID NANOSCALE ELECTRONIC DEVICES; SILICON NANOWIRES; THERMOELECTRIC FIGURE;
CARBON NANOTUBES; TRANSPORT-COEFFICIENTS; SIMULATION; GERMANIUM; GE; SI;
HETEROSTRUCTURES
AB Low-dimensional nanostructured materials show large variations in their thermal transport properties. In this work, we investigate the influence of the core-shell architecture on nanowire (1D) thermal conductivity and evaluate its validity as a strategy to achieve a better thermoelectric performance. To obtain the thermal conductivity values, equilibrium molecular dynamics simulations are conducted for core-shell nanowires of silicon and germanium. To explore the parameter space, we have calculated thermal conductivity values of the Si-core/Ge-shell and Ge-core/Si-shell nanowires having different cross-sectional sizes and core contents at several temperatures. Our results indicate that (1) increasing the cross-sectional area of pristine Si and pristine Ge nanowires increases the thermal conductivity, (2) increasing the Ge core size in the Ge-core/Si-shell structure results in a decrease in the thermal conductivity at 300 K, (3) the thermal conductivity of the Sicore/Ge-shell nanowires demonstrates a minima at a specific core size, (4) no significant variation in the thermal conductivity is observed in nanowires for temperatures larger than 300 K, and (5) the predicted thermal conductivity within the frame of applied geometrical constraints is found to be around 10 W/(mK) for the Si and Ge core-shell architecture with a smooth interface. The value is still higher than the amorphous limit (1 W/(mK)). This represents a significant reduction in thermal conductivity with respect to their bulk crystalline and pristine nanowire forms. Furthermore, we observed additional suppression of thermal conductivity through the introduction of interface roughness to Si/Ge core-shell nanowires. Published by AIP Publishing.
C1 [Sarikurt, S.; Kinaci, A.; Cagin, T.] Texas A&M Univ, Dept Mat Sci & Engn, College Stn, TX 77843 USA.
[Sarikurt, S.] Dokuz Eylul Univ, Fac Sci, Dept Phys, TR-35390 Izmir, Turkey.
[Ozden, A.; Kandemir, A.] Anadolu Univ, Fac Engn, Dept Mat Sci & Engn, TR-26555 Eskisehir, Turkey.
[Sevik, C.] Anadolu Univ, Fac Engn, Dept Mech Engn, TR-26555 Eskisehir, Turkey.
[Kinaci, A.] Argonne Natl Lab, Ctr Nanoscale Mat, Lemont, IL 60439 USA.
[Haskins, J. B.] NASA, AMA Inc, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Haskins, J. B.; Cagin, T.] Texas A&M Univ, Artie McFerrin Dept Chem Engn, College Stn, TX 77843 USA.
RP Cagin, T (reprint author), Texas A&M Univ, Dept Mat Sci & Engn, College Stn, TX 77843 USA.; Cagin, T (reprint author), Texas A&M Univ, Artie McFerrin Dept Chem Engn, College Stn, TX 77843 USA.
EM sevil.sarikurt@deu.edu.tr; csevik@anadolu.edu.tr; tcagin@tamu.edu
RI Kandemir, Ali/A-4034-2017
OI Kandemir, Ali/0000-0001-9813-6421
FU International Institute of Materials for Energy Conversion (IIMEC) at
Texas AM University; NSF International Materials Institute [DMR
0844082]; Scientific and Technological Research Council of Turkey
(TUBITAK-BIDEB) [2219]; Scientific and Technological Research Council of
Turkey [TUBITAK-113F096]; Anadolu University [BAP-140717335]; Turkish
Academy of Sciences (TUBA-GEBIP)
FX We acknowledge support from the International Institute of Materials for
Energy Conversion (IIMEC) at Texas A&M University, an NSF International
Materials Institute (DMR 0844082). All of the computations were carried
out at the facilities of Laboratory of Computational Engineering of
Nanomaterials, Chemical Engineering Cluster, Supercomputing Center of
Texas A&M University, and also Eskisehir Anadolu University. S. Sarikurt
was supported by Scientific and Technological Research Council of Turkey
(TUBITAK-BIDEB) 2219 International Postdoctoral Research Scholarship
Program and IIMEC during this study at Texas A&M University, C. Sevik
acknowledges the support from Scientific and Technological Research
Council of Turkey (TUBITAK-113F096), Anadolu University (BAP-140717335),
and Turkish Academy of Sciences (TUBA-GEBIP) to this project.
NR 52
TC 1
Z9 1
U1 5
U2 10
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-8979
EI 1089-7550
J9 J APPL PHYS
JI J. Appl. Phys.
PD APR 21
PY 2016
VL 119
IS 15
AR 155101
DI 10.1063/1.4946835
PG 9
WC Physics, Applied
SC Physics
GA DQ1WS
UT WOS:000378991800031
ER
PT J
AU Crear, DP
Lawson, DD
Seminoff, JA
Eguchi, T
LeRoux, RA
Lowe, CG
AF Crear, Daniel P.
Lawson, Daniel D.
Seminoff, Jeffrey A.
Eguchi, Tomoharu
LeRoux, Robin A.
Lowe, Christopher G.
TI Seasonal shifts in the movement and distribution of green sea turtles
Chelonia mydas in response to anthropogenically altered water
temperatures
SO MARINE ECOLOGY PROGRESS SERIES
LA English
DT Article
DE Thermal refuge; Ectotherm; Warm water effluent; Power plants; Acoustic
telemetry; Foraging aggregation
ID GULF-OF-CALIFORNIA; MARINE-ENVIRONMENT; SCALE MOVEMENTS; FORAGING AREA;
GROWTH-RATES; MODELS; FLORIDA; LAGOON; DORMANCY; ECOLOGY
AB Anthropogenically altered water temperatures (AAWT) have the potential to affect the movement and distribution of marine ectothermic species. Green sea turtles (GSTs) Chelonia mydas are an ectothermic species observed inhabiting 2 sites with AAWT at the northern point of their geographical range in the eastern Pacific. An acoustic receiver array was deployed with temperature loggers at the San Gabriel River, Long Beach, CA, where 2 power plants discharge warm water into the river, and at the 7th St. Basin, Seal Beach, CA, a dredged shallow basin with warmer water compared to surrounding coastal habitats during the summer months. Juvenile GSTs (n = 22, straight carapace length = 45.2 to 96.8 cm) were tagged with acoustic transmitters. Turtles in the basin migrated into the river during winter months when temperatures dropped below 15 degrees C. During the winter, turtles were most frequently detected at the river receiver stations adjacent to and downstream of the power plants. This suggests that GSTs use the warm effluent as a thermal refuge, avoiding colder areas upstream of the power plants and near the river mouth. In the summer, turtles were most frequently detected at receiver stations upstream of the power plants, potentially exploiting areas of the river with higher primary productivity. AAWT sustain the northernmost aggregation of GSTs in the eastern Pacific year round; however, based on GST thermal tolerance, this population is expected to change their movement patterns when the power plants discontinue discharging warm water by 2029.
C1 [Crear, Daniel P.] Coll William & Mary, Virginia Inst Marine Sci, POB 1346, Gloucester Point, VA 23062 USA.
[Lawson, Daniel D.] NOAA, Protected Resources Div, West Coast Reg Off, Natl Marine Fisheries Serv, 501 West Ocean Blvd,Suite 4200, Long Beach, CA 90802 USA.
[Seminoff, Jeffrey A.; Eguchi, Tomoharu; LeRoux, Robin A.] NOAA, Protected Resources Div, Southwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, 8901 La Jolla Shores Dr, La Jolla, CA 92037 USA.
[Lowe, Christopher G.] Calif State Univ Long Beach, Dept Biol Sci, 1250 Bellflower Blvd, Long Beach, CA 90840 USA.
RP Crear, DP (reprint author), Coll William & Mary, Virginia Inst Marine Sci, POB 1346, Gloucester Point, VA 23062 USA.
EM dcrear8@gmail.com
FU NOAA Fisheries West Coast Regional Office; SCTC Marine Biology
Foundation; Los Angeles Rod and Reel Club
FX Financial support was provided by the NOAA Fisheries West Coast Regional
Office, SCTC Marine Biology Foundation, and the Los Angeles Rod and Reel
Club. We thank US Fish and Wildlife manager K. Gilligan, US Navy
Ecologist B. Schallmann, and Los Cerritos Wetlands for logical support.
We also thank the following individuals for their support in the field:
D. Prosperi, J. Schumacher, B. MacDonald, and the entire NOAA-NMFS team
that assisted with turtle capture. We especially thank numerous
volunteers who helped with data-collection, including J. Hinricher, A.
Jimenez, C. White, and W. Stahnke. We particularly thank D. Johnson, J.
Archie, and T. Fahy for their input and guidance during the project. All
research and animal handling was carried out under the National Marine
Fisheries Service Permit #14510
NR 47
TC 1
Z9 1
U1 17
U2 28
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 0171-8630
EI 1616-1599
J9 MAR ECOL PROG SER
JI Mar. Ecol.-Prog. Ser.
PD APR 21
PY 2016
VL 548
BP 219
EP 232
DI 10.3354/meps11696
PG 14
WC Ecology; Marine & Freshwater Biology; Oceanography
SC Environmental Sciences & Ecology; Marine & Freshwater Biology;
Oceanography
GA DM5GF
UT WOS:000376375000016
ER
PT J
AU Sainio, S
Nordlund, D
Caro, MA
Gandhiraman, R
Koehne, J
Wester, N
Koskinen, J
Meyyappan, M
Laurila, T
AF Sainio, S.
Nordlund, D.
Caro, M. A.
Gandhiraman, R.
Koehne, J.
Wester, N.
Koskinen, J.
Meyyappan, M.
Laurila, T.
TI Correlation between sp(3)-to-sp(2) Ratio and Surface Oxygen
Functionalities in Tetrahedral Amorphous Carbon (ta-C) Thin Film
Electrodes and Implications of Their Electrochemical Properties
SO JOURNAL OF PHYSICAL CHEMISTRY C
LA English
DT Article
ID X-RAY-ABSORPTION; PYROLYTIC-GRAPHITE ELECTRODE; DIAMOND SURFACES; NEXAFS
SPECTROSCOPY; FINE-STRUCTURE; ASCORBIC-ACID; EXCITATION; REDUCTION;
MECHANISM; DOPAMINE
AB Detailed information about the physicochemical properties of a given surface is important in order to understand and predict the performance of materials in electrochemical applications. Here we present a detailed X-ray absorption spectroscopy study of two different tetrahedral amorphous-carbon (ta-C) thin films and their subsequent electrochemical characterization. The results show marked differences in ta-C surface and bulk properties, namely differences in the amount of surface functional groups and their sp(3)/sp(2) ratios, respectively. In particular, the variation in the oxygen content of the surface leads to significantly different behavior in electrochemical measurements, such as a 10-fold increase in sensitivity for dopamine and stronger response to ascorbic acid. Results of the surface properties were further analyzed by simulations carried out within the framework of density functional theory (DFT) as well as by utilizing Raman spectroscopy.
C1 [Sainio, S.; Caro, M. A.; Laurila, T.] Aalto Univ, Sch Elect Engn, Dept Elect Engn & Automat, Espoo 02150, Finland.
[Nordlund, D.] SLAC Natl Accelerator Lab, Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA 94025 USA.
[Caro, M. A.] Aalto Univ, Sch Sci, Dept Appl Phys, COMP Ctr Excellence Computat Nanosci, Espoo 02150, Finland.
[Gandhiraman, R.; Koehne, J.; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Wester, N.; Koskinen, J.] Aalto Univ, Sch Chem Technol, Dept Mat Sci, Espoo 02150, Finland.
RP Laurila, T (reprint author), Aalto Univ, Sch Elect Engn, Dept Elect Engn & Automat, Espoo 02150, Finland.
EM tomi.laurila@aalto.fi
RI Koskinen, Jari/J-3886-2014; Laurila, Tomi/B-2076-2013; Nordlund,
Dennis/A-8902-2008
OI Nordlund, Dennis/0000-0001-9524-6908
FU Academy of Finland [285015, 285526]
FX T.L. and S.S. acknowledge funding from Academy of Finland (Grant Numbers
285015 and 285526). M.A.C. would like to acknowledge the computational
resources provided for this project by Aalto University's Science IT
project through the Triton cluster, and helpful comments on XAS spectra
and ARS calculations from Arto Sakko and Toma Susi.
NR 41
TC 2
Z9 2
U1 5
U2 7
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1932-7447
J9 J PHYS CHEM C
JI J. Phys. Chem. C
PD APR 21
PY 2016
VL 120
IS 15
BP 8298
EP 8304
DI 10.1021/acs.jpcc.6b02342
PG 7
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA DK3IU
UT WOS:000374811100045
ER
PT J
AU Boyajian, TS
LaCourse, DM
Rappaport, SA
Fabrycky, D
Fischer, DA
Gandolfi, D
Kennedy, GM
Korhonen, H
Liu, MC
Moor, A
Olah, K
Vida, K
Wyatt, MC
Best, WMJ
Brewer, J
Ciesla, F
Csak, B
Deeg, HJ
Dupuy, TJ
Handler, G
Heng, K
Howell, SB
Ishikawa, ST
Kovacs, J
Kozakis, T
Kriskovics, L
Lehtinen, J
Lintott, C
Lynn, S
Nespral, D
Nikbakhsh, S
Schawinski, K
Schmitt, JR
Smith, AM
Szabo, G
Szabo, R
Viuho, J
Wang, J
Weiksnar, A
Bosch, M
Connors, JL
Goodman, S
Green, G
Hoekstra, AJ
Jebson, T
Jek, KJ
Omohundro, MR
Schwengeler, HM
Szewczyk, A
AF Boyajian, T. S.
LaCourse, D. M.
Rappaport, S. A.
Fabrycky, D.
Fischer, D. A.
Gandolfi, D.
Kennedy, G. M.
Korhonen, H.
Liu, M. C.
Moor, A.
Olah, K.
Vida, K.
Wyatt, M. C.
Best, W. M. J.
Brewer, J.
Ciesla, F.
Csak, B.
Deeg, H. J.
Dupuy, T. J.
Handler, G.
Heng, K.
Howell, S. B.
Ishikawa, S. T.
Kovacs, J.
Kozakis, T.
Kriskovics, L.
Lehtinen, J.
Lintott, C.
Lynn, S.
Nespral, D.
Nikbakhsh, S.
Schawinski, K.
Schmitt, J. R.
Smith, A. M.
Szabo, Gy.
Szabo, R.
Viuho, J.
Wang, J.
Weiksnar, A.
Bosch, M.
Connors, J. L.
Goodman, S.
Green, G.
Hoekstra, A. J.
Jebson, T.
Jek, K. J.
Omohundro, M. R.
Schwengeler, H. M.
Szewczyk, A.
TI Planet Hunters IX. KIC 8462852-where's the flux?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE comets: general; planets and satellites: dynamical evolution and
stability; stars: activity; stars: individual: KIC 8462852; stars:
peculiar
ID INFRARED FILTER SET; BETA-PICTORIS; SOLAR-SYSTEM; DEBRIS DISKS;
IRREGULAR SATELLITES; CIRCUMSTELLAR DISK; INTRINSIC COLORS;
MAIN-SEQUENCE; ARCHIVE DATA; AA TAURI
AB Over the duration of the Kepler mission, KIC 8462852 was observed to undergo irregularly shaped, aperiodic dips in flux of up to similar to 20 per cent. The dipping activity can last for between 5 and 80 d. We characterize the object with high-resolution spectroscopy, spectral energy distribution fitting, radial velocity measurements, high-resolution imaging, and Fourier analyses of the Kepler light curve. We determine that KIC 8462852 is a typical main-sequence F3 V star that exhibits no significant IR excess, and has no very close interacting companions. In this paper, we describe various scenarios to explain the dipping events observed in the Kepler light curve. We confirm that the dipping signals in the data are not caused by any instrumental or data processing artefact, and thus are astrophysical in origin. We construct scenario-independent constraints on the size and location of a body in the system that are needed to reproduce the observations. We deliberate over several assorted stellar and circumstellar astrophysical scenarios, most of which have problems explaining the data in hand. By considering the observational constraints on dust clumps in orbit around a normal main-sequence star, we conclude that the scenario most consistent with the data in hand is the passage of a family of exocomet or planetesimal fragments, all of which are associated with a single previous break-up event, possibly caused by tidal disruption or thermal processing. The minimum total mass associated with these fragments likely exceeds 10(-6) M-circle plus, corresponding to an original rocky body of > 100 km in diameter. We discuss the necessity of future observations to help interpret the system.
C1 [Boyajian, T. S.; Fischer, D. A.; Brewer, J.; Schmitt, J. R.; Wang, J.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[LaCourse, D. M.; Bosch, M.; Connors, J. L.; Goodman, S.; Green, G.; Hoekstra, A. J.; Jebson, T.; Jek, K. J.; Omohundro, M. R.; Schwengeler, H. M.; Szewczyk, A.] Amateur Astronomer, Helsinki, Finland.
[Rappaport, S. A.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Rappaport, S. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Fabrycky, D.] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA.
[Gandolfi, D.] Univ Turin, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy.
[Gandolfi, D.] Heidelberg Univ, Zentrum Astron, Landessternwarte Konigstuhl, Konigstuhl 12, D-69117 Heidelberg, Germany.
[Kennedy, G. M.; Wyatt, M. C.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Korhonen, H.] Univ Turku, Finnish Ctr Astron ESO FINCA, Vaisalantie 20, FI-21500 Turku, Finland.
[Korhonen, H.] Univ Copenhagen, Niels Bohr Inst, Ctr Star & Planet Format, Oster Voldgade 5-7, DK-1350 Copenhagen, Denmark.
[Liu, M. C.; Best, W. M. J.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Moor, A.; Olah, K.; Vida, K.; Kriskovics, L.; Szabo, Gy.; Szabo, R.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Th M ut 15 17, H-1121 Budapest, Hungary.
[Ciesla, F.] Univ Chicago, Dept Geophys Sci, 5734 South Ellis Ave, Chicago, IL 60637 USA.
[Csak, B.; Kovacs, J.] ELTE Gothard Astrophys Observ, Szent Imre Herceg Ut 112, H-9704 Szombathely, Hungary.
[Deeg, H. J.; Nespral, D.] Inst Astrofis Canarias, C Via Lactea S-N, E-38205 Tenerife, Spain.
[Deeg, H. J.] Univ La Laguna, Dept Astrofis, E-38200 Tenerife, Spain.
[Dupuy, T. J.] Univ Texas Austin, Dept Astron, 2515 Speedway C1400, Austin, TX 78712 USA.
[Handler, G.] Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland.
[Heng, K.] Univ Bern, Ctr Space & Habitabil, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Howell, S. B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ishikawa, S. T.; Weiksnar, A.] Adler Planetarium, Dept Citizen Sci, 1300 S Lake Shore Dr, Chicago, IL 60605 USA.
[Kozakis, T.] Cornell Univ, Carl Sagan Inst, Ithaca, NY 14853 USA.
[Lehtinen, J.; Nikbakhsh, S.; Viuho, J.] Univ Helsinki, Dept Phys, POB 64, FI-00014 Helsinki, Finland.
[Lintott, C.] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
[Lynn, S.] CartoDB, 247 Ctr St, New York, NY 10013 USA.
[Nikbakhsh, S.] Finnish Meteorol Inst, POB 503, FI-00101 Helsinki, Finland.
[Schawinski, K.] ETH, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Smith, A. M.] GitHub Inc, 88 Colin P Kelly Jr St, San Francisco, CA 94107 USA.
[Szabo, Gy.] Gothard Lendulet Res Team, Szent Imre Herceg Ut 112, H-9704 Szombathely, Hungary.
[Wang, J.] CALTECH, Pasadena, CA 91109 USA.
RI Korhonen, Heidi/E-3065-2016;
OI Korhonen, Heidi/0000-0003-0529-1161; Fabrycky,
Daniel/0000-0003-3750-0183; Brewer, John/0000-0002-9873-1471; Gandolfi,
Davide/0000-0001-8627-9628
FU NASA [ADAP12-0172, ADAP14-0245]; European Union through ERC [279973];
Hungarian Research Grants [OTKA K-109276, OTKA K-113117]; Hungarian
Academy of Sciences [LP2012-31]; Hungarian National Research,
Development and Innovation Office - NKFIH [K-115709]; ESA PECS Contract
[4000110889/14/NL/NDe]; Momentum grant of the MTA CSFK Lendulet Disc
Research Group; Polish NCN [2011/01/B/ST9/05448]; NSF [AST-0407380,
AST-0909073, AST-1313370, AST-0909222]; European Community [269194,
312844]; Swiss National Science Foundation [PP00P2_138979/1]; State for
RDi (MINECO) [AYA2012-39346-C02-02]; National Aeronautics and Space
Administration
FX TSB acknowledges support provided through NASA grant ADAP12-0172 and
ADAP14-0245. MCW and GMK acknowledge the support of the European Union
through ERC grant number 279973. The authors acknowledge support from
the Hungarian Research Grants OTKA K-109276, OTKA K-113117, the
Lendulet-2009 and Lendulet-2012 Program (LP2012-31) of the Hungarian
Academy of Sciences, the Hungarian National Research, Development and
Innovation Office - NKFIH K-115709, and the ESA PECS Contract No.
4000110889/14/NL/NDe. This work was supported by the Momentum grant of
the MTA CSFK Lendulet Disc Research Group. GH acknowledges support by
the Polish NCN grant 2011/01/B/ST9/05448. Based on observations made
with the NOT, operated by the Nordic Optical Telescope Scientific
Association at the Observatorio del Roque de los Muchachos, La Palma,
Spain, of the Instituto de Astrofisica de Canarias. This research made
use of The DASCH project; we are also grateful for partial support from
NSF grants AST-0407380, AST-0909073, and AST-1313370. The research
leading to these results has received funding from the European
Community's Seventh Framework Programme (FP7/2007-2013) under grant
agreements no. 269194 (IRSES/ASK) and no. 312844 (SPACEINN). We thank
Scott Dahm, Julie Rivera, and the Keck Observatory staff for their
assistance with these observations. This research was supported in part
by NSF grant AST-0909222 awarded to M. Liu. The authors wish to
recognize and acknowledge the very significant cultural role and
reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. KS gratefully
acknowledges support from Swiss National Science Foundation Grant
PP00P2_138979/1. HJD and DN acknowledge support by grant
AYA2012-39346-C02-02 of the Spanish Secretary of State for R&D&i
(MINECO). This paper makes use of data from the first public release of
the WASP data (Butters et al. 2010) as provided by the WASP consortium
and services at the NASA Exoplanet Archive, which is operated by the
California Institute of Technology, under contract with the National
Aeronautics and Space Administration under the Exoplanet Exploration
Program. This publication makes use of data products from the Wide-field
Infrared Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, and NEOWISE, which is a project of the Jet
Propulsion Laboratory/California Institute of Technology. WISE and
NEOWISE are funded by the National Aeronautics and Space Administration.
This research made use of the SIMBAD and VIZIER Astronomical Databases,
operated at CDS, Strasbourg, France (http://cdsweb.u-strasbg.fr/), and
of NASA's Astrophysics Data System.
NR 86
TC 20
Z9 20
U1 5
U2 12
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 21
PY 2016
VL 457
IS 4
BP 3988
EP 4004
DI 10.1093/mnras/stw218
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6CE
UT WOS:000373586000043
ER
PT J
AU Shvartzvald, Y
Maoz, D
Udalski, A
Sumi, T
Friedmann, M
Kaspi, S
Poleski, R
Szymanski, MK
Skowron, J
Kozlowski, S
Wyrzykowski, L
Mroz, P
Pietrukowicz, P
Pietrzynski, G
Soszynski, I
Ulaczyk, K
Abe, F
Barry, RK
Bennett, DP
Bhattacharya, A
Bond, IA
Freeman, M
Inayama, K
Itow, Y
Koshimoto, N
Ling, CH
Masuda, K
Fukui, A
Matsubara, Y
Muraki, Y
Ohnishi, K
Rattenbury, NJ
Saito, T
Sullivan, DJ
Suzuki, D
Tristram, PJ
Wakiyama, Y
Yonehara, A
AF Shvartzvald, Y.
Maoz, D.
Udalski, A.
Sumi, T.
Friedmann, M.
Kaspi, S.
Poleski, R.
Szymanski, M. K.
Skowron, J.
Kozlowski, S.
Wyrzykowski, L.
Mroz, P.
Pietrukowicz, P.
Pietrzynski, G.
Soszynski, I.
Ulaczyk, K.
Abe, F.
Barry, R. K.
Bennett, D. P.
Bhattacharya, A.
Bond, I. A.
Freeman, M.
Inayama, K.
Itow, Y.
Koshimoto, N.
Ling, C. H.
Masuda, K.
Fukui, A.
Matsubara, Y.
Muraki, Y.
Ohnishi, K.
Rattenbury, N. J.
Saito, To.
Sullivan, D. J.
Suzuki, D.
Tristram, P. J.
Wakiyama, Y.
Yonehara, A.
CA Wise Observ Grp
Optical Gravitational Lens Expt
Microlensing Observations
TI The frequency of snowline-region planets from four years of
OGLE-MOA-Wise second-generation microlensing
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: micro; surveys; binaries: general; planetary
systems; Galaxy: stellar content
ID GRAVITATIONAL LENSING EXPERIMENT; BROWN DWARF DESERT; EXTRASOLAR
PLANETS; GALACTIC BULGE; MASS; EVENTS; SYSTEMS; STARS;
MOA-2011-BLG-293LB; MULTIPLICITY
AB We present a statistical analysis of the first four seasons from a 'second-generation' microlensing survey for extrasolar planets, consisting of near-continuous time coverage of 8 deg(2) of the Galactic bulge by the Optical Gravitational Lens Experiment (OGLE), Microlensing Observations in Astrophysics (MOA), and Wise microlensing surveys. During this period, 224 microlensing events were observed by all three groups. Over 12 per cent of the events showed a deviation from single-lens microlensing, and for similar to one-third of those the anomaly is likely caused by a planetary companion. For each of the 224 events, we have performed numerical ray-tracing simulations to calculate the detection efficiency of possible companions as a function of companion-to-host mass ratio and separation. Accounting for the detection efficiency, we find that 55(-22)(+34) per cent of microlensed stars host a snowline planet. Moreover, we find that Neptune-mass planets are similar to 10 times more common than Jupiter-mass planets. The companion-to-host mass-ratio distribution shows a deficit at q similar to 10(-2), separating the distribution into two companion populations, analogous to the stellar-companion and planet populations, seen in radial-velocity surveys around solar-like stars. Our survey, however, which probes mainly lower mass stars, suggests a minimum in the distribution in the super-Jupiter mass range, and a relatively high occurrence of brown-dwarf companions.
C1 [Shvartzvald, Y.; Maoz, D.; Friedmann, M.; Kaspi, S.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Udalski, A.; Szymanski, M. K.; Skowron, J.; Kozlowski, S.; Wyrzykowski, L.; Mroz, P.; Pietrukowicz, P.; Pietrzynski, G.; Soszynski, I.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland.
[Sumi, T.; Koshimoto, N.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Poleski, R.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
[Ulaczyk, K.] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England.
[Abe, F.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Wakiyama, Y.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Barry, R. K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Bennett, D. P.; Bhattacharya, A.; Suzuki, D.] Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA.
[Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Private Bag 102-904, Auckland, New Zealand.
[Freeman, M.; Rattenbury, N. J.] Univ Auckland, Dept Phys, Private Bag 92-019, Auckland 1001, New Zealand.
[Inayama, K.; Yonehara, A.] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan.
[Yonehara, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan.
[Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand.
[Tristram, P. J.] Mt John Univ Observ, POB 56, Lake Tekapo 8770, New Zealand.
RP Shvartzvald, Y (reprint author), Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
EM yossishv@gmail.com
RI Skowron, Jan/M-5186-2014
OI Skowron, Jan/0000-0002-2335-1730
FU I-CORE programme of the Planning and Budgeting Committee; Israel Science
Foundation [1829/12]; US-Israel Binational Science Foundation; National
Science Centre, Poland [MAESTRO 2014/14/A/ST9/00121]; JSPS
[JSPS23103002, JSPS24253004, JSPS26247023]; [JSPS25103508]; [23340064]
FX We thank T. Mazeh and the anonymous referee for useful comments and
discussions. This research was supported by the I-CORE programme of the
Planning and Budgeting Committee and the Israel Science Foundation,
Grant 1829/12. DM acknowledges support by the US-Israel Binational
Science Foundation. The OGLE project has received funding from the
National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to
AU. TS acknowledges the financial support from the JSPS, JSPS23103002,
JSPS24253004 and JSPS26247023. The MOA project is supported by the grant
JSPS25103508 and 23340064.
NR 41
TC 12
Z9 12
U1 1
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 21
PY 2016
VL 457
IS 4
BP 4089
EP 4113
DI 10.1093/mnras/stw191
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6CE
UT WOS:000373586000051
ER
PT J
AU Harris, K
Farrah, D
Schulz, B
Hatziminaoglou, E
Viero, M
Anderson, N
Bethermin, M
Chapman, S
Clements, DL
Cooray, A
Efstathiou, A
Feltre, A
Hurley, P
Ibar, E
Lacy, M
Oliver, S
Page, MJ
Perez-Fournon, I
Petty, SM
Pitchford, LK
Rigopoulou, D
Scott, D
Symeonidis, M
Vieira, J
Wang, LY
AF Harris, Kathryn
Farrah, Duncan
Schulz, Bernhard
Hatziminaoglou, Evanthia
Viero, Marco
Anderson, Nick
Bethermin, Matthieu
Chapman, Scott
Clements, David L.
Cooray, Asantha
Efstathiou, Andreas
Feltre, Anne
Hurley, Peter
Ibar, Eduardo
Lacy, Mark
Oliver, Sebastian
Page, Mathew J.
Perez-Fournon, Ismael
Petty, Sara M.
Pitchford, Lura K.
Rigopoulou, Dimitra
Scott, Douglas
Symeonidis, Myrto
Vieira, Joaquin
Wang, Lingyu
TI Star formation rates in luminous quasars at 2 < z < 3
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; quasars: general; galaxies: starburst; galaxies:
star formation; infrared: galaxies
ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS;
DIGITAL-SKY-SURVEY; BLACK-HOLE ACCRETION; ULTRALUMINOUS INFRARED
GALAXIES; SDSS STRIPE 82; OSCILLATION SPECTROSCOPIC SURVEY;
SUBMILLIMETER NUMBER COUNTS; RADIATIVE-TRANSFER MODELS; EMISSION-LINE
PROPERTIES
AB We investigate the relation between star formation rates ((M) over dot(s)) and AGN properties in optically selected type 1 quasars at 2 < z < 3 using data from Herschel and the SDSS. We find that (M) over dot(s) remains approximately constant with redshift, at 300 +/- 100 M-circle dot yr(-1). Conversely, (M) over dot(s) increases with AGN luminosity, up to a maximum of similar to 600 M-circle dot yr(-1), and with CIV FWHM. In context with previous results, this is consistent with a relation between (M) over dot(s) and black hole accretion rate ((M) over dot(bh)) existing in only parts of the z - (M) over dot(s) - (M) over dot(bh) plane, dependent on the free gas fraction, the trigger for activity, and the processes that may quench star formation. The relations between (M) over dot(s) and both AGN luminosity and C IV FWHM are consistent with star formation rates in quasars scaling with black hole mass, though we cannot rule out a separate relation with black hole accretion rate. Star formation rates are observed to decline with increasing CIV equivalent width. This decline can be partially explained via the Baldwin effect, but may have an additional contribution from one or more of three factors; M-i is not a linear tracer of L-2500, the Baldwin effect changes form at high AGN luminosities, and high C IV EW values signpost a change in the relation between (M) over dot(s) and (M) over dot(bh). Finally, there is no strong relation between (M) over dot(s) and Eddington ratio, or the asymmetry of the C IV line. The former suggests that star formation rates do not scale with how efficiently the black hole is accreting, while the latter is consistent with C IV asymmetries arising from orientation effects.
C1 [Harris, Kathryn; Farrah, Duncan; Anderson, Nick; Petty, Sara M.; Pitchford, Lura K.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Harris, Kathryn; Perez-Fournon, Ismael] Inst Astrofis Canarias, C Via Lactea S-N, E-38205 Tenerife, Spain.
[Harris, Kathryn; Perez-Fournon, Ismael] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Schulz, Bernhard] CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Schulz, Bernhard] JPL, CALTECH, Ctr Infrared Proc & Anal, MS 100-22, Pasadena, CA 91125 USA.
[Hatziminaoglou, Evanthia; Bethermin, Matthieu; Pitchford, Lura K.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Viero, Marco] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 382 Via Pueblo Mall, Stanford, CA 94305 USA.
[Chapman, Scott] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
[Clements, David L.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England.
[Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Efstathiou, Andreas] European Univ Cyprus, Sch Sci, Diogenes St, CY-1516 Nicosia, Cyprus.
[Feltre, Anne] UPMC, Univ Paris 04, CNRS, Inst Astrophys Paris,UMR7095, F-75014 Paris, France.
[Hurley, Peter; Oliver, Sebastian] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Ibar, Eduardo] Univ Valparaiso, Inst Fis & Astron, Avda Gran Bretana 1111, Valparaiso, Chile.
[Lacy, Mark] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
[Page, Mathew J.; Symeonidis, Myrto] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
[Rigopoulou, Dimitra] Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England.
[Scott, Douglas] Univ British Columbia, Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
[Vieira, Joaquin] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Vieira, Joaquin] Univ Illinois, Dept Phys, 1002 W Green St, Urbana, IL 61801 USA.
[Wang, Lingyu] SRON Netherlands Inst Space Res, Landleven 12, NL-9747 AD Groningen, Netherlands.
[Wang, Lingyu] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
RP Harris, K; Farrah, D (reprint author), Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.; Harris, K (reprint author), Inst Astrofis Canarias, C Via Lactea S-N, E-38205 Tenerife, Spain.; Harris, K (reprint author), Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
EM kateharris142@gmail.com; dfarrah@gmail.com
OI Scott, Douglas/0000-0002-6878-9840
FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France);
ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA
(USA); Alfred P. Sloan Foundation; National Science Foundation; U.S.
Department of Energy Office of Science; University of Arizona; Brazilian
Participation Group; Brookhaven National Laboratory; Carnegie Mellon
University; University of Florida; French Participation Group; German
Participation Group; Harvard University; Instituto de Astrofisica de
Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns
Hopkins University; Lawrence Berkeley National Laboratory; Max Planck
Institute for Astrophysics; Max Planck Institute for Extraterrestrial
Physics; New Mexico State University; New York University; Ohio State
University; Pennsylvania State University; University of Portsmouth;
Princeton University; Spanish Participation Group; University of Tokyo;
University of Utah; Vanderbilt University; University of Virginia;
University of Washington; Yale University; ERC [321323-NEOGAL]
FX We thank the referee for a very helpful report. Herschel is an ESA space
observatory with instruments provided by European-led Principal
Investigator consortia and with participation from NASA. The Herschel
spacecraft was designed, built, tested, and launched under a contract to
ESA managed by the Herschel/Planck Project team by an industrial
consortium under the overall responsibility of the prime contractor
Thales Alenia Space (Cannes), and including Astrium (Friedrichshafen)
responsible for the payload module and for system testing, Thales Alenia
Space (Turin) responsible for the service module, and Astrium (Toulouse)
responsible for the telescope, with in excess of a hundred
subcontractors. SPIRE has been developed by a consortium of institutes
led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC
(China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain);
Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL,
UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA).
This development has been supported by national funding agencies: CSA
(Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN
(Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). Funding for
SDSS-III has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, and the
U.S. Department of Energy Office of Science. SDSS-III is managed by the
Astrophysical Research Consortium for the Participating Institutions of
the SDSS-III Collaboration including the University of Arizona, the
Brazilian Participation Group, Brookhaven National Laboratory, Carnegie
Mellon University, University of Florida, the French Participation
Group, the German Participation Group, Harvard University, the Instituto
de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA
Participation Group, Johns Hopkins University, Lawrence Berkeley
National Laboratory, Max Planck Institute for Astrophysics, Max Planck
Institute for Extraterrestrial Physics, New Mexico State University, New
York University, Ohio State University, Pennsylvania State University,
University of Portsmouth, Princeton University, the Spanish
Participation Group, University of Tokyo, University of Utah, Vanderbilt
University, University of Virginia, University of Washington, and Yale
University. AF acknowledges support from the ERC via an Advanced Grant
321323-NEOGAL.
NR 154
TC 5
Z9 5
U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 21
PY 2016
VL 457
IS 4
BP 4179
EP 4194
DI 10.1093/mnras/stw286
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6CE
UT WOS:000373586000057
ER
PT J
AU Southworth, J
Tregloan-Reed, J
Andersen, MI
Novati, SC
Ciceri, S
Colque, JP
D'Ago, G
Dominik, M
Evans, DF
Gu, SH
Herrera-Cordova, A
Hinse, TC
Jorgensen, UG
Juncher, D
Kuffmeier, M
Mancini, L
Peixinho, N
Popovas, A
Rabus, M
Skottfelt, J
Tronsgaard, R
Unda-Sanzana, E
Wang, XB
Wertz, O
Alsubai, KA
Andersen, JM
Bozza, V
Bramich, DM
Burgdorf, M
Damerdji, Y
Diehl, C
Elyiv, A
Jaimes, RF
Haugbolle, T
Hundertmark, M
Kains, N
Kerins, E
Korhonen, H
Liebig, C
Mathiasen, M
Penny, MT
Rahvar, S
Scarpetta, G
Schmidt, RW
Snodgrass, C
Starkey, D
Surdej, J
Vilela, C
von Essen, C
Wang, Y
AF Southworth, John
Tregloan-Reed, J.
Andersen, M. I.
Novati, S. Calchi
Ciceri, S.
Colque, J. P.
D'Ago, G.
Dominik, M.
Evans, D. F.
Gu, S. -H.
Herrera-Cordova, A.
Hinse, T. C.
Jorgensen, U. G.
Juncher, D.
Kuffmeier, M.
Mancini, L.
Peixinho, N.
Popovas, A.
Rabus, M.
Skottfelt, J.
Tronsgaard, R.
Unda-Sanzana, E.
Wang, X. -B.
Wertz, O.
Alsubai, K. A.
Andersen, J. M.
Bozza, V.
Bramich, D. M.
Burgdorf, M.
Damerdji, Y.
Diehl, C.
Elyiv, A.
Jaimes, R. Figuera
Haugbolle, T.
Hundertmark, M.
Kains, N.
Kerins, E.
Korhonen, H.
Liebig, C.
Mathiasen, M.
Penny, M. T.
Rahvar, S.
Scarpetta, G.
Schmidt, R. W.
Snodgrass, C.
Starkey, D.
Surdej, J.
Vilela, C.
von Essen, C.
Wang, Y.
TI High-precision photometry by telescope defocussing - VIII. WASP-22,
WASP-41, WASP-42 and WASP-55
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: fundamental parameters; stars: individual: WASP-22, WASP-41,
WASP-42, WASP-55; planetary systems
ID TRANSITING EXTRASOLAR PLANETS; STELLAR EVOLUTION DATABASE; SPIN-ORBIT
ALIGNMENT; HOT JUPITER PLANET; LIGHT-CURVE; EXOPLANETARY SYSTEM;
PHYSICAL-PROPERTIES; GIANT PLANETS; STARSPOTS; STAR
AB We present 13 high-precision and four additional light curves of four bright southern-hemisphere transiting planetary systems: WASP-22, WASP-41, WASP-42 and WASP-55. In the cases of WASP-42 and WASP-55, these are the first follow-up observations since their discovery papers. We present refined measurements of the physical properties and orbital ephemerides of all four systems. No indications of transit timing variations were seen. All four planets have radii inflated above those expected from theoretical models of gas-giant planets; WASP-55 b is the most discrepant with a mass of 0.63M(Jup) and a radius of 1.34 R-Jup. WASP-41 shows brightness anomalies during transit due to the planet occulting spots on the stellar surface. Two anomalies observed 3.1 d apart are very likely due to the same spot. We measure its change in position and determine a rotation period for the host star of 18.6 +/- 1.5 d, in good agreement with a published measurement from spot-induced brightness modulation, and a sky-projected orbital obliquity of lambda = 6 +/- 11 degrees. We conclude with a compilation of obliquity measurements from spot-tracking analyses and a discussion of this technique in the study of the orbital configurations of hot Jupiters.
C1 [Southworth, John; Evans, D. F.; Vilela, C.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Tregloan-Reed, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Andersen, M. I.; Korhonen, H.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
[Novati, S. Calchi] CALTECH, Exoplanet Sci Inst, NASA, MS 100-22, Pasadena, CA 91125 USA.
[Novati, S. Calchi; Bozza, V.] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo 2 132, I-84084 Fisciano, SA, Italy.
[Novati, S. Calchi; D'Ago, G.; Scarpetta, G.] IIASS, I-84019 Vietri Sul Mare, SA, Italy.
[Ciceri, S.; Mancini, L.; Rabus, M.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Colque, J. P.; Herrera-Cordova, A.; Peixinho, N.; Unda-Sanzana, E.] Univ Antofagasta, Fac Ciencias Basicas, Unidad Astron, Ave U Antofagasta, Antofagasta 02800, Chile.
[Dominik, M.; Jaimes, R. Figuera; Liebig, C.; Starkey, D.] Univ St Andrews, Sch Phys & Astron, SUPA, North Haugh, St Andrews KY16 9SS, Fife, Scotland.
[Gu, S. -H.; Wang, X. -B.; Wang, Y.] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China.
[Gu, S. -H.; Wang, X. -B.] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Peoples R China.
[Hinse, T. C.] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea.
[Jorgensen, U. G.; Juncher, D.; Kuffmeier, M.; Popovas, A.; Skottfelt, J.; Andersen, J. M.; Haugbolle, T.; Hundertmark, M.; Korhonen, H.; Mathiasen, M.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Jorgensen, U. G.; Juncher, D.; Kuffmeier, M.; Popovas, A.; Skottfelt, J.; Andersen, J. M.; Haugbolle, T.; Hundertmark, M.; Korhonen, H.; Mathiasen, M.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Mancini, L.] INAF, Osservatorio Astron Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy.
[Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Skottfelt, J.] Open Univ, Dept Phys Sci, Ctr Elect Imaging, Milton Keynes MK7 6AA, Bucks, England.
[Tronsgaard, R.; von Essen, C.] Aarhus Univ, Dept Phys & Astron, SAC, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
[Wertz, O.; Damerdji, Y.; Elyiv, A.; Surdej, J.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Alsubai, K. A.; Bramich, D. M.] Qatar Fdn, QEERI, HBKU, POB 5825, Doha, Qatar.
[Andersen, J. M.] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA.
[Bozza, V.; Scarpetta, G.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy.
[Burgdorf, M.] Univ Hamburg, Inst Meteorol, Bundesstr 55, D-20146 Hamburg, Germany.
[Diehl, C.; Schmidt, R. W.] Heidelberg Univ, Astron Rech Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany.
[Diehl, C.] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Elyiv, A.] Univ Bologna, Dipartmento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Elyiv, A.] Ukrainian Acad Sci, Main Astron Observ, Vul Akad Zabolotnoho 27, UA-03680 Kiev, Ukraine.
[Jaimes, R. Figuera] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Kains, N.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Kerins, E.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England.
[Korhonen, H.] Univ Turku, Finnish Ctr Astron ESO FINCA, Vaisalantie 20, FI-21500 Piikkio, Finland.
[Penny, M. T.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, POB 111559161, Tehran, Iran.
[Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England.
RP Southworth, J (reprint author), Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
EM astro.js@keele.ac.uk
RI Korhonen, Heidi/E-3065-2016; Hundertmark, Markus/C-6190-2015; D'Ago,
Giuseppe/N-8318-2016;
OI Korhonen, Heidi/0000-0003-0529-1161; Hundertmark,
Markus/0000-0003-0961-5231; D'Ago, Giuseppe/0000-0001-9697-7331;
Dominik, Martin/0000-0002-3202-0343; Tronsgaard,
Rene/0000-0003-1001-0707; Wang, Yi-Bo/0000-0002-5172-8558; Penny,
Matthew/0000-0001-7506-5640
FU Danish Council for Independent Research, Natural Sciences (FNU);
Leverhulme Trust; ORAU (Oak Ridge Associated Universities); NASA; UK's
Science and Technology Facilities Council; CONICYT QUIMAL [130004];
Danish National Research Foundation [DNRF106]; ASTERISK project
(ASTERoseismic Investigations with SONG and Kepler) - European Research
Council [267864]; KASI [2012-1-410-02, 2013-9-400-00, 2014-1-400-06,
2015-1-850-04]; Gemini-Conicyt Fund [32120036]; Regione Campania from
POR-FSE Campania; Communaute francaise de Belgique - Actions de
recherche concertees - Academie Wallonie-Europe
FX This study is based on data collected by MiNDSTEp with the Danish 1.54 m
telescope at the ESO La Silla Observatory. The operation of the Danish
1.54-m telescope is financed by a grant to UGJ from the Danish Council
for Independent Research, Natural Sciences (FNU). The reduced light
curves presented in this work will be made available at the CDS
(http://vizier.u-strasbg.fr/) and at http://www.astro.keele.ac.uk/jkt/.
We thank Laetitia Delrez and Marion Neveu-VanMalle for providing
published light curves of WASP-41. J So acknowledges financial support
from the Leverhulme Trust in the form of a Philip Leverhulme Prize. JTR
acknowledges financial support from ORAU (Oak Ridge Associated
Universities) and NASA in the form of a NASA Post-Doctoral Programme
(NPP) Fellowship. DFE is funded by the UK's Science and Technology
Facilities Council. EU-S acknowledges the support of CONICYT QUIMAL
130004 project. Funding for the Stellar Astrophysics Centre in Aarhus is
provided by The Danish National Research Foundation (grant agreement no.
DNRF106). The research is supported by the ASTERISK project
(ASTERoseismic Investigations with SONG and Kepler) funded by the
European Research Council (grant agreement no. 267864). TCH acknowledges
KASI research grants #2012-1-410-02, #2013-9-400-00, #2014-1-400-06 and
#2015-1-850-04. NP acknowledges funding by the Gemini-Conicyt Fund,
allocated to project no. 32120036. GD acknowledges Regione Campania for
support from POR-FSE Campania 2014-2020. YD, AE, OW and J Su acknowledge
support from the Communaute francaise de Belgique - Actions de recherche
concertees - Academie Wallonie-Europe. The following internet-based
resources were used in research for this paper: the ESO Digitized Sky
Survey; the NASA Astrophysics Data System; the SIMBAD data base and
VizieR catalogue access tool operated at CDS, Strasbourg, France; and
the ar chi iv scientific paper preprint service operated by Cornell
University.
NR 60
TC 0
Z9 0
U1 3
U2 5
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 21
PY 2016
VL 457
IS 4
BP 4205
EP 4217
DI 10.1093/mnras/stw279
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6CE
UT WOS:000373586000059
ER
PT J
AU Bonamente, M
Nevalainen, J
Tilton, E
Liivamagi, J
Tempel, E
Heinamaki, P
Fang, T
AF Bonamente, M.
Nevalainen, J.
Tilton, E.
Liivamaegi, J.
Tempel, E.
Heinamaki, P.
Fang, T.
TI A possible Chandra and Hubble Space Telescope detection of extragalactic
WHIM towards PG 1116+215
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE quasars: individual: PG 1116+215; large-scale structure of Universe
ID HOT INTERGALACTIC MEDIUM; X-RAY-ABSORPTION; LY-ALPHA FOREST;
PHYSICAL-PROPERTIES; SCULPTOR WALL; 1ES 1553+113; SIGHT LINE; BARYONS;
ABSORBERS; GALAXIES
AB We have analysed Chandra low energy transmission grating and XMM-Newton Reflection Grating Spectrometer (RGS) spectra towards the z = 0.177 quasar PG 1116+215, a sightline that is rendered particularly interesting by the Hubble Space Telescope (HST) detection of several OVI and HI broad Lyman alpha absorption (BLA) lines that may be associated with the warm-hot intergalactic medium (WHIM). We performed a search for resonance K alpha absorption lines from OVII and OVIII at the redshifts of the detected far-ultraviolet lines. We detected an absorption line in the Chandra spectra at the 5.2 sigma confidence level at wavelengths corresponding to OVIII K alpha at z = 0.0911 +/- 0.0004 +/- 0.0005 (statistical followed by systematic error). This redshift is within 3 sigma of that of an HI broad Lyman alpha of b similar or equal to 130 km s(-1) (corresponding to a temperature of log T(K) similar or equal to 6.1) at z = 0.092 79 +/- 0.000 05. We have also analysed the available XMM-Newton RGS data towards PG 1116+215. Unfortunately, the XMM-Newton data are not suitable to investigate this line because of instrumental features at the wavelengths of interest. At the same redshift, the Chandra and XMM-Newton spectra have OVII K alpha absorption-line features of significance 1.5 sigma and 1.8 sigma, respectively. We also analysed the available Sloan Digital Sky Survey (SDSS) spectroscopic galaxy survey data towards PG 1116+215 in the redshift range of interest. We found evidence for a galaxy filament that intersect the PG 1116+215 sightline and additional galaxy structures that may host WHIM. The HI BLA and the OVIII K alpha absorbers are within a few Mpc of the filament (assuming that redshifts track Hubble flow distances) or consistent with gas accreting on to the filament from either direction relative to the sightline with velocities of a few x 100 km s(-1). The combination of HST, Chandra, XMM-Newton and SDSS data indicates that we have likely detected a multi-temperature WHIM at z similar or equal to 0.091-0.093 towards PG 1116+215. The OVIII Ka absorption line indicates gas at high temperature, log T(K) >= 6.4, with a total column density of the order of log N-H(cm(2)) >= 20 and a baryon overdensity delta(b) similar to 100-1000 for sightline lengths of L = 1-10 Mpc. This detection highlights the importance of BLA absorption lines as possible signposts of high-temperature WHIM filaments.
C1 [Bonamente, M.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Bonamente, M.] NASA, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA.
[Nevalainen, J.; Liivamaegi, J.; Tempel, E.] Tartu Observ, Observatooriumi 1, EE-61602 Toravere, Estonia.
[Tilton, E.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA, Boulder, CO 80309 USA.
[Heinamaki, P.] Tuorla Observ, Vaisalantie 20, FI-21500 Piikkio, Finland.
[Fang, T.] Xiamen Univ, Dept Astron, Xiamen 361005, Fujian, Peoples R China.
[Fang, T.] Xiamen Univ, Inst Theoret Phys & Astrophys, Xiamen 361005, Fujian, Peoples R China.
RP Bonamente, M (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.; Bonamente, M (reprint author), NASA, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA.
EM bonamem@uah.edu
FU Estonian Research Council [PUT246]; National Natural Science Foundation
of China [11273021]; Estonian Ministry of Education and Research
[IUT26-2, IUT40-2]; NASA/MSFC
FX JN is funded by PUT246 grant from Estonian Research Council. We thank Dr
M. Weisskopf and Prof. A. Finoguenov for help in the interpretation of
the data. TF was partially supported by the National Natural Science
Foundation of China under grant No. 11273021. ET and JT acknowledge the
support by institutional research funding IUT26-2, IUT40-2 of the
Estonian Ministry of Education and Research. MB acknowledges support by
the NASA/MSFC 2015 Faculty Fellow programme.
NR 38
TC 2
Z9 2
U1 3
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 21
PY 2016
VL 457
IS 4
BP 4236
EP 4247
DI 10.1093/mnras/stw285
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6CE
UT WOS:000373586000061
ER
PT J
AU Caballero, RN
Lee, KJ
Lentati, L
Desvignes, G
Champion, DJ
Verbiest, JPW
Janssen, GH
Stappers, BW
Kramer, M
Lazarus, P
Possenti, A
Tiburzi, C
Perrodin, D
Oslowski, S
Babak, S
Bassa, CG
Brem, P
Burgay, M
Cognard, I
Gair, JR
Graikou, E
Guillemot, L
Hessels, JWT
Karuppusamy, R
Lassus, A
Liu, K
Mckee, J
Mingarelli, CMF
Petiteau, A
Purver, MB
Rosado, PA
Sanidas, S
Sesana, A
Shaifullah, G
Smits, R
Taylor, SR
Theureau, G
van Haasteren, R
Vecchio, A
AF Caballero, R. N.
Lee, K. J.
Lentati, L.
Desvignes, G.
Champion, D. J.
Verbiest, J. P. W.
Janssen, G. H.
Stappers, B. W.
Kramer, M.
Lazarus, P.
Possenti, A.
Tiburzi, C.
Perrodin, D.
Oslowski, S.
Babak, S.
Bassa, C. G.
Brem, P.
Burgay, M.
Cognard, I.
Gair, J. R.
Graikou, E.
Guillemot, L.
Hessels, J. W. T.
Karuppusamy, R.
Lassus, A.
Liu, K.
McKee, J.
Mingarelli, C. M. F.
Petiteau, A.
Purver, M. B.
Rosado, P. A.
Sanidas, S.
Sesana, A.
Shaifullah, G.
Smits, R.
Taylor, S. R.
Theureau, G.
van Haasteren, R.
Vecchio, A.
TI The noise properties of 42 millisecond pulsars from the European Pulsar
Timing Array and their impact on gravitational-wave searches
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational waves; methods: data analysis; pulsars: general
ID RADIO ASTRONOMICAL POLARIMETRY; BLACK-HOLE BINARIES; RELATIVISTIC
GRAVITY; COMPACT BINARIES; SINGLE-PULSE; PRECISION; RADIATION; LIMITS;
VARIABILITY; DISPERSION
AB The sensitivity of Pulsar Timing Arrays to gravitational waves (GWs) depends on the noise present in the individual pulsar timing data. Noise may be either intrinsic or extrinsic to the pulsar. Intrinsic sources of noise will include rotational instabilities, for example. Extrinsic sources of noise include contributions from physical processes which are not sufficiently well modelled, for example, dispersion and scattering effects, analysis errors and instrumental instabilities. We present the results from a noise analysis for 42 millisecond pulsars (MSPs) observed with the European Pulsar Timing Array. For characterizing the low-frequency, stochastic and achromatic noise component, or 'timing noise', we employ two methods, based on Bayesian and frequentist statistics. For 25 MSPs, we achieve statistically significant measurements of their timing noise parameters and find that the two methods give consistent results. For the remaining 17 MSPs, we place upper limits on the timing noise amplitude at the 95 per cent confidence level. We additionally place an upper limit on the contribution to the pulsar noise budget from errors in the reference terrestrial time standards (below 1 per cent), and we find evidence for a noise component which is present only in the data of one of the four used telescopes. Finally, we estimate that the timing noise of individual pulsars reduces the sensitivity of this data set to an isotropic, stochastic GW background by a factor of > 9.1 and by a factor of > 2.3 for continuous GWs from resolvable, inspiralling supermassive black hole binaries with circular orbits.
C1 [Caballero, R. N.; Lee, K. J.; Desvignes, G.; Champion, D. J.; Verbiest, J. P. W.; Kramer, M.; Lazarus, P.; Tiburzi, C.; Oslowski, S.; Graikou, E.; Karuppusamy, R.; Lassus, A.; Liu, K.; Mingarelli, C. M. F.; Shaifullah, G.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Lee, K. J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Lentati, L.] Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England.
[Verbiest, J. P. W.; Tiburzi, C.; Oslowski, S.; Shaifullah, G.] Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany.
[Janssen, G. H.; Bassa, C. G.; Hessels, J. W. T.; Smits, R.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Janssen, G. H.; Stappers, B. W.; Kramer, M.; McKee, J.; Purver, M. B.; Sanidas, S.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Possenti, A.; Perrodin, D.; Burgay, M.] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy.
[Babak, S.; Brem, P.; Sesana, A.] Albert Einstein Inst, Max Planck Inst Gravitationsphys, Muhlenberg 1, D-14476 Golm, Germany.
[Cognard, I.; Guillemot, L.; Theureau, G.] Univ Orleans, CNRS, Lab Phys & Chim Environm & Espace, F-45071 Orleans, France.
[Cognard, I.; Guillemot, L.; Theureau, G.] CNRS INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France.
[Gair, J. R.] Univ Edinburgh, Sch Math, Kings Bldg, Edinburgh EH9 3JZ, Midlothian, Scotland.
[Hessels, J. W. T.; Sanidas, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Mingarelli, C. M. F.] CALTECH, TAPIR, MC 350-17, Pasadena, CA 91125 USA.
[Petiteau, A.] Univ Paris 07, APC UFR Phys, Batiment Condorcet, F-75205 Paris 13, France.
[Rosado, P. A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia.
[Rosado, P. A.] Albert Einstein Inst, Max Planck Inst Gravitationsphys, Callinstr 38, D-30167 Hannover, Germany.
[Sesana, A.; Vecchio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Taylor, S. R.; van Haasteren, R.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91106 USA.
[Theureau, G.] Univ Paris Diderot, CNRS INSU, Observ Paris, Lab Univ & Theories LUTh, 5 Pl Jules Janssen, F-92190 Meudon, France.
RP Caballero, RN (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM caball@mpifr-bonn.mpg.de
RI Perrodin, Delphine/L-1916-2016; Vecchio, Alberto/F-8310-2015;
OI Perrodin, Delphine/0000-0002-1806-2483; Vecchio,
Alberto/0000-0002-6254-1617; Taylor, Stephen/0000-0003-0264-1453; McKee,
James/0000-0002-2885-8485; Oslowski, Stefan/0000-0003-0289-0732
FU 'Programme National de Cosmologie and Galaxies' (PNCG) of CNRS/INSU,
France; STFC in the UK; Netherlands Foundation for Scientific Research
NWO; International Max Planck Research School Bonn/Cologne; Bonn-Cologne
Graduate School; National Basic Research Program of China, 973 Program
[2015CB857101]; NSFC [11373011]; Alexander von Humboldt Foundation; NWO;
European Research Council under the European Union / ERC [337062];
European Community; Royal Society; NASA; NASA [PF3-140116]
FX Part of this work is based on observations with the 100-m telescope of
the Max-Planck-Institut fur Radioastronomie (MPIfR) at Effelsberg. The
Nancay Radio Observatory is operated by the Paris Observatory,
associated with the French Centre National de la Recherche Scientifique
(CNRS). We acknowledge financial support from 'Programme National de
Cosmologie and Galaxies' (PNCG) of CNRS/INSU, France. Pulsar research at
the Jodrell Bank Centre for Astrophysics and the observations using the
Lovell Telescope is supported by a consolidated grant from the STFC in
the UK. The Westerbork Synthesis Radio Telescope is operated by the
Netherlands Institute for Radio Astronomy (ASTRON) with support from The
Netherlands Foundation for Scientific Research NWO.; RNC acknowledges
the support of the International Max Planck Research School Bonn/Cologne
and the Bonn-Cologne Graduate School. KJL gratefully acknowledge support
from National Basic Research Program of China, 973 Program, 2015CB857101
and NSFC 11373011. PL acknowledges the support of the International Max
Planck Research School Bonn/Cologne. SO is supported by the Alexander
von Humboldt Foundation. JWTH acknowledges funding from an NWO Vidi
fellowship and from the European Research Council under the European
Union's Seventh Framework Programme (FP/2007-2013) / ERC Starting Grant
agreement no. 337062 ('DRAGNET'). CMFM was supported by a Marie Curie
International Outgoing Fellowship within the 7th European Community
Framework Programme. AS is supported by the Royal Society. This research
was in part supported by ST's appointment to the NASA Postdoctoral
Program at the Jet Propulsion Laboratory, administered by Oak Ridge
Associated Universities through a contract with NASA. RvH is supported
by NASA Einstein Fellowship grant PF3-140116.
NR 72
TC 4
Z9 4
U1 1
U2 8
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 21
PY 2016
VL 457
IS 4
BP 4421
EP 4440
DI 10.1093/mnras/stw179
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6CE
UT WOS:000373586000075
ER
PT J
AU Archer, A
Benbow, W
Bird, R
Buchovecky, M
Buckley, JH
Bugaev, V
Byrum, K
Cardenzana, JV
Cerruti, M
Chen, X
Ciupik, L
Collins-Hughes, E
Connolly, MP
Eisch, JD
Falcone, A
Feng, Q
Finley, JP
Fleischhack, H
Flinders, A
Fortson, L
Furniss, A
Gillanders, GH
Griffin, S
Grube, J
Gyuk, G
Hakansson, N
Hanna, D
Holder, J
Humensky, TB
Hutten, M
Johnson, CA
Kaaret, P
Kar, P
Kelley-Hoskins, N
Kertzman, M
Kieda, D
Krause, M
Krennrich, F
Kumar, S
Lang, MJ
McArthur, S
McCann, A
Meagher, K
Millis, J
Moriarty, P
Mukherjee, R
Nieto, D
Ong, RA
Park, N
Pelassa, V
Pohl, M
Popkow, A
Pueschel, E
Quinn, J
Ragan, K
Ratliff, G
Reynolds, PT
Richards, GT
Roache, E
Rousselle, J
Santander, M
Sembroski, GH
Shahinyan, K
Smith, AW
Staszak, D
Telezhinsky, I
Tucci, JV
Tyler, J
Vassiliev, VV
Wakely, SP
Weiner, OM
Weinstein, A
Wilhelm, A
Williams, DA
Zitzer, B
Yusef-Zadeh, F
AF Archer, A.
Benbow, W.
Bird, R.
Buchovecky, M.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cardenzana, J. V.
Cerruti, M.
Chen, X.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Eisch, J. D.
Falcone, A.
Feng, Q.
Finley, J. P.
Fleischhack, H.
Flinders, A.
Fortson, L.
Furniss, A.
Gillanders, G. H.
Griffin, S.
Grube, J.
Gyuk, G.
Hakansson, N.
Hanna, D.
Holder, J.
Humensky, T. B.
Huetten, M.
Johnson, C. A.
Kaaret, P.
Kar, P.
Kelley-Hoskins, N.
Kertzman, M.
Kieda, D.
Krause, M.
Krennrich, F.
Kumar, S.
Lang, M. J.
McArthur, S.
McCann, A.
Meagher, K.
Millis, J.
Moriarty, P.
Mukherjee, R.
Nieto, D.
Ong, R. A.
Park, N.
Pelassa, V.
Pohl, M.
Popkow, A.
Pueschel, E.
Quinn, J.
Ragan, K.
Ratliff, G.
Reynolds, P. T.
Richards, G. T.
Roache, E.
Rousselle, J.
Santander, M.
Sembroski, G. H.
Shahinyan, K.
Smith, A. W.
Staszak, D.
Telezhinsky, I.
Tucci, J. V.
Tyler, J.
Vassiliev, V. V.
Wakely, S. P.
Weiner, O. M.
Weinstein, A.
Wilhelm, A.
Williams, D. A.
Zitzer, B.
Yusef-Zadeh, F.
TI TEV GAMMA-RAY OBSERVATIONS OF THE GALACTIC CENTER RIDGE BY VERITAS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: center; gamma rays: general; supernovae: individual (G0.9+0.1)
ID SGR-A-ASTERISK; SAGITTARIUS B2 CLOUD; CENTER BLACK-HOLE; HIGH-ENERGY;
CENTER REGION; MOLECULAR CLOUDS; CHANDRA OBSERVATIONS; STELLAR CLUSTERS;
EMISSION; TELESCOPE
AB The Galactic Center ridge has been observed extensively in the past by both GeV and TeV gamma-ray instruments revealing a wealth of structure, including a diffuse component and the point sources G0.9+0.1 (a composite supernova remnant) and Sgr A* (believed to be associated with the supermassive black hole located at the center of our Galaxy). Previous very high energy (VHE) gamma-ray observations with the H.E.S.S.. experiment have also detected an extended TeV gamma-ray component along the Galactic plane in the >300 GeV gamma-ray regime. Here we report on observations of the Galactic Center ridge from 2010 to 2014 by the VERITAS telescope array in the >2 TeV energy range. From these observations we (1) provide improved measurements of the differential energy spectrum for Sgr A* in the >2 TeV gamma-ray regime, (2) provide a detection in the >2 TeV gamma-ray emission from the composite SNR G0.9+0.1 and an improved determination of its multi-TeV gamma-ray energy spectrum, and. (3) report on the detection of VER J1746-289, a localized enhancement of >2 TeV gamma-ray emission along the Galactic plane.
C1 [Archer, A.; Buckley, J. H.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Cerruti, M.; Pelassa, V.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Bird, R.; Collins-Hughes, E.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Buchovecky, M.; Ong, R. A.; Popkow, A.; Rousselle, J.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Byrum, K.; Zitzer, B.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Cardenzana, J. V.; Eisch, J. D.; Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Chen, X.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Chen, X.; Fleischhack, H.; Huetten, M.; Kelley-Hoskins, N.; Krause, M.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] DESY, Platanenallee 6, D-15738 Zeuthen, Germany.
[Ciupik, L.; Grube, J.; Gyuk, G.; Ratliff, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Feng, Q.; Finley, J. P.; McArthur, S.; Sembroski, G. H.; Tucci, J. V.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
[Flinders, A.; Kar, P.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Furniss, A.] Calif State Univ East Bay, Dept Phys, Hayward, CA 94542 USA.
[Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
[Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Humensky, T. B.; Nieto, D.; Weiner, O. M.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Meagher, K.; Richards, G. T.] Georgia Inst Technol, Sch Phys, 837 State St NW, Atlanta, GA 30332 USA.
[Meagher, K.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA.
[Millis, J.] Anderson Univ, Dept Phys, 1100 East 5th St, Anderson, IN 46012 USA.
[Mukherjee, R.; Santander, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Sci, Cork, Ireland.
[Smith, A. W.] Univ Maryland, College Pk, MD 20742 USA.
[Smith, A. W.] NASA, Goddard Space Flight Ctr, College Pk, MD 20742 USA.
[Yusef-Zadeh, F.] Northwestern Univ, Dept Phys & Astron, CIERA, Evanston, IL 60208 USA.
RP Smith, AW (reprint author), Univ Maryland, College Pk, MD 20742 USA.; Smith, AW (reprint author), NASA, Goddard Space Flight Ctr, College Pk, MD 20742 USA.
EM asmith44@umd.edu
OI Chen, Xuhui/0000-0002-9745-0248; Krause, Maria/0000-0001-7595-0914
FU U.S. Department of Energy Office of Science; U.S. National Science
Foundation; Smithsonian Institution; NSERC in Canada; Cycle 7 Fermi
Guest Investigator program [NNH13ZDA001N]
FX This research is supported by grants from the U.S. Department of Energy
Office of Science, the U.S. National Science Foundation, and the
Smithsonian Institution and by NSERC in Canada. We acknowledge the
excellent work of the technical support staff at the Fred Lawrence
Whipple Observatory and at the collaborating institutions in the
construction and operation of the instrument.; A.W.S. acknowledges
support through the Cycle 7 Fermi Guest Investigator program, grant
number NNH13ZDA001N.
NR 58
TC 2
Z9 2
U1 3
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2016
VL 821
IS 2
AR 129
DI 10.3847/0004-637X/821/2/129
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DN5JM
UT WOS:000377102700058
ER
PT J
AU Deck, KM
Agol, E
AF Deck, Katherine M.
Agol, Eric
TI TRANSIT TIMING VARIATIONS FOR PLANETS NEAR ECCENTRICITY-TYPE MEAN MOTION
RESONANCES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE celestial mechanics; planets and satellites: dynamical evolution and
stability; planets and satellites: fundamental parameters
ID MASS; EXOPLANETS; DENSITIES; PAIR
AB We derive the transit timing variations (TTVs) of two planets near a second-order mean motion resonance (MMR) on nearly circular orbits. We show that the TTVs of each planet are given by sinusoids with a frequency of jn(2) - (j - 2)n(1), where j >= 3 is an integer characterizing the resonance and n(2) and n(1) are the mean motions of the outer and inner planets, respectively. The amplitude of the TTV depends on the mass of the perturbing planet, relative to the mass of the star, and on both the eccentricities and longitudes of pericenter of each planet. The TTVs of the two planets are approximated anti-correlated, with phases of phi and approximate to phi + pi, where the phase phi also depends on the eccentricities and longitudes of pericenter. Therefore, the TTVs caused by proximity to a second-order MMR do not in general uniquely determine both planet masses, eccentricities, and pericenters. This is completely analogous to the case of TTVs induced by two planets near a first-order MMR. We explore how other TTV signals, such as the short-period synodic TTV or a first-order resonant TTV, in combination with the second-order resonant TTV, can break degeneracies. Finally, we derive approximate formulae for the TTVs of planets near any order eccentricity-type MMR; this shows that the same basic sinusoidal TTV structure holds for all eccentricity-type resonances. Our general formula reduces to previously derived results near first-order MMRs.
C1 [Deck, Katherine M.] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Agol, Eric] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA.
RP Deck, KM (reprint author), CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM kdeck@caltech.edu
OI /0000-0002-0802-9145
FU JCPA postdoctoral fellowship at Caltech; NASA [NNX13AF20G, NNX13AF62G,
NNH05ZDA001C]; NASA Astrobiology Institutes Virtual Planetary Laboratory
FX We would like to thank the referee who helped us to clarify and improve
this document. K.D. acknowledges support from the JCPA postdoctoral
fellowship at Caltech. E.A. acknowledges support from NASA grants
NNX13AF20G, NNX13AF62G, and NASA Astrobiology Institutes Virtual
Planetary Laboratory, supported by NASA under cooperative agreement
NNH05ZDA001C.
NR 24
TC 3
Z9 3
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2016
VL 821
IS 2
AR 96
DI 10.3847/0004-637X/821/2/96
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DN5JM
UT WOS:000377102700025
ER
PT J
AU Okuzumi, S
Momose, M
Sirono, S
Kobayashi, H
Tanaka, H
AF Okuzumi, Satoshi
Momose, Munetake
Sirono, Sin-iti
Kobayashi, Hiroshi
Tanaka, Hidekazu
TI SINTERING-INDUCED DUST RING FORMATION IN PROTOPLANETARY DISKS:
APPLICATION TO THE HL TAU DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; planets and satellites: composition; protoplanetary
disks; stars: individual (HL Tau); submillimeter: planetary systems
ID HEAD-ON COLLISIONS; PLANETESIMAL FORMATION; SOLAR NEBULA; SIZE
DISTRIBUTION; SNOW LINE; GAS DISKS; MAGNETOROTATIONAL-INSTABILITY;
GRAVITATIONAL-INSTABILITY; MILLIMETER WAVELENGTHS; NUMERICAL-SIMULATION
AB The latest observation of HL Tau by ALMA revealed spectacular concentric dust rings in its circumstellar disk. We attempt to explain the multiple ring structure as a consequence of aggregate sintering. Sintering is known to reduce the sticking efficiency of dust aggregates and occurs at temperatures slightly below the sublimation point of the constituent material. We present a dust growth model that incorporates sintering and use it to simulate global dust evolution due to sintering, coagulation, fragmentation, and radial inward drift in a modeled HL Tau disk. We show that aggregates consisting of multiple species of volatile ices experience sintering, collisionally disrupt, and pile up at multiple locations slightly outside the snow lines of the volatiles. At wavelengths of 0.87-1.3 mm, these sintering zones appear as bright, optically thick rings with a spectral slope of approximate to 2, whereas the non-sintering zones appear as darker, optically thinner rings of a spectral slope of approximate to 2.3-2.5. The observational features of the sintering and non-sintering zones are consistent with those of the major bright and dark rings found in the HL Tau disk, respectively. Radial pileup and vertical settling occur simultaneously if disk turbulence is weak and if monomers constituting the aggregates are similar to 1 mu m in radius. For the radial gas temperature profile of T = 310(r/1 au)(-0.57) K, our model perfectly reproduces the brightness temperatures of the optically thick bright rings and reproduces their orbital distances to an accuracy of less than or similar to 30%.
C1 [Okuzumi, Satoshi] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Okuzumi, Satoshi] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Momose, Munetake] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Sirono, Sin-iti] Nagoya Univ, Dept Earth & Environm Sci, Nagoya, Aichi 4648601, Japan.
[Kobayashi, Hiroshi] Nagoya Univ, Dept Phys, Nagoya, Aichi 4648602, Japan.
[Tanaka, Hidekazu] Hokkaido Univ, Inst Low Temp Sci, Sapporo, Hokkaido 0600819, Japan.
RP Okuzumi, S (reprint author), Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.; Okuzumi, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM okuzumi@geo.titech.ac.jp
RI Tanaka, Hidekazu/E-1226-2012
OI Tanaka, Hidekazu/0000-0001-9659-658X
FU MEXT of Japan [23103004, 23103005, 25400447, 26287101, 15H02065];
Astrobiology Center Project of National Institutes of Natural Sciences
(NINS) [AB271020]
FX The authors thank Neal Turner for discussions on the temperature
distribution of the HL Tau disk, and Akimasa Kataoka for useful comments
on the modeling of aggregate porosity. We also thank Takashi Tsukagoshi,
Tetsuya Hama, Misato Fukagawa, Hideko Nomura, and Mario Flock for
comments and discussions, and the anonymous referee for prompt and
constructive comments. This work is supported by Grants-in-Aid for
Scientific Research (nos. 23103004, 23103005, 25400447, 26287101,
15H02065) from MEXT of Japan and by the Astrobiology Center Project of
National Institutes of Natural Sciences (NINS) (grant no. AB271020).
This paper makes use of the following ALMA data: ADS/JAO.
ALMA#2011.0.00015. SV. ALMA is a partnership of ESO (representing its
member states), NSF (USA) and NINS (Japan), together with NRC (Canada),
NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation
with the Republic of Chile. The Joint ALMA Observatory is operated by
ESO, AUI/NRAO, and NAOJ.
NR 118
TC 16
Z9 16
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2016
VL 821
IS 2
AR 82
DI 10.3847/0004-637X/821/2/82
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DN5JM
UT WOS:000377102700011
ER
PT J
AU Quintana, EV
Barclay, T
Borucki, WJ
Rowe, JF
Chambers, JE
AF Quintana, Elisa V.
Barclay, Thomas
Borucki, William J.
Rowe, Jason F.
Chambers, John E.
TI THE FREQUENCY OF GIANT IMPACTS ON EARTH-LIKE WORLDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; methods: numerical; planetary systems; planets
and satellites: dynamical evolution and stability; planets and
satellites: formation; planets and satellites: terrestrial planets
ID TERRESTRIAL PLANET FORMATION; BINARY STAR SYSTEMS; N-BODY SIMULATIONS;
LOW-MASS STARS; SYMPLECTIC INTEGRATOR; PROTOPLANETARY DISK; CLOSE
ENCOUNTERS; FORMING IMPACT; SOLAR NEBULA; ACCRETION
AB The late stages of terrestrial planet formation are dominated by giant impacts that collectively influence the growth, composition, and habitability of any planets that form. Hitherto, numerical models designed to explore these late stage collisions have been limited by assuming that all collisions lead to perfect accretion, and many of these studies lack the large number of realizations needed to account for the chaotic nature of N-body systems. We improve on these limitations by performing 280 simulations of planet formation around a Sun-like star, half of which used an N-body algorithm that has recently been modified to include fragmentation and hit-and-run (bouncing) collisions. We find that when fragmentation is included, the final planets formed are comparable in terms of mass and number; however, their collision histories differ significantly and the accretion time approximately doubles. We explored impacts onto Earth-like planets, which we parameterized in terms of their specific impact energies. Only 15 of our 164 Earth-analogs experienced an impact that was energetic enough to strip an entire atmosphere. To strip about half of an atmosphere requires energies comparable to recent models of the Moon-forming giant impact. Almost all Earth-analogs received at least one impact that met this criteria during the 2 Gyr simulations and the median was three giant impacts. The median time of the final giant impact was 43 Myr after the start of the simulations, leading us to conclude that the time-frame of the Moon-forming impact is typical among planetary systems around Sun-like stars.
C1 [Quintana, Elisa V.; Barclay, Thomas; Borucki, William J.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas] Bay Area Environm Res Inst, 625 2nd St,Ste 209, Petaluma, CA 94952 USA.
[Rowe, Jason F.] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
[Chambers, John E.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
RP Quintana, EV (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
FU NASA Senior Fellowship at the Ames Research Center; NASA
FX The authors would like to thank Jack Lissauer, Billy Quarles, Chris
Henze, Simon Lock, and Sarah Stewart for comments that greatly improved
this manuscript. E.V.Q. is supported by a NASA Senior Fellowship at the
Ames Research Center, administered by Oak Ridge Associated Universities
through a contract with NASA. The simulations presented here were
performed using the Pleiades Supercomputer provided by the NASA High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at Ames Research Center.
NR 70
TC 1
Z9 1
U1 2
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2016
VL 821
IS 2
AR 126
DI 10.3847/0004-637X/821/2/126
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DN5JM
UT WOS:000377102700055
ER
PT J
AU Rana, V
Loh, A
Corbel, S
Tomsick, JA
Chakrabarty, D
Walton, DJ
Barret, D
Boggs, SE
Christensen, FE
Craig, W
Fuerst, F
Gandhi, P
Grefenstette, BW
Hailey, C
Harrison, FA
Madsen, KK
Rahoui, F
Stern, D
Tendulkar, S
Zhang, WW
AF Rana, Vikram
Loh, Alan
Corbel, Stephane
Tomsick, John A.
Chakrabarty, Deepto
Walton, Dominic J.
Barret, Didier
Boggs, Steven E.
Christensen, Finn E.
Craig, William
Fuerst, Felix
Gandhi, Poshak
Grefenstette, Brian W.
Hailey, Charles
Harrison, Fiona A.
Madsen, Kristin K.
Rahoui, Farid
Stern, Daniel
Tendulkar, Shriharsh
Zhang, William W.
TI CHARACTERIZING X-RAY AND RADIO EMISSION IN THE BLACK HOLE X-RAY BINARY
V404 CYGNI DURING QUIESCENCE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; stars: black holes; stars: individual (V404
Cyg); X-rays: binaries
ID ADVECTION-DOMINATED ACCRETION; COMPACT JET; GX 339-4;
INFRARED-SPECTROSCOPY; EVENT HORIZONS; MODEL; TRANSIENTS; TELESCOPE;
SPECTRUM; ARRAY
AB We present results from multi-wavelength simultaneous X-ray and radio observations of the black hole X-ray binary V404. Cyg in quiescence. Our coverage with NuSTAR provides the very first opportunity to study the X-ray spectrum of V404. Cyg at energies above 10 keV. The unabsorbed broadband (0.3-30 keV) quiescent luminosity of the source is 8.9 x 10(32) erg s(-1) for a distance of 2.4 kpc. The source shows clear variability on short timescales (an hour to a couple of hours) in the. radio, soft X-ray, and hard X-ray bands in the form of multiple flares. The broadband X-ray spectra obtained from XMM-Newton and NuSTAR can be characterized with a power-law model having a photon index of Gamma = 2.12 +/- 0.07 (90% confidence errors); however, residuals at high energies indicate spectral curvature significant at a 3 sigma confidence level with the. e-folding energy of the cutoff as 20(-7)(+20) keV. Such curvature can be explained using synchrotron emission from the base of a jet outflow. Radio observations using the VLA reveal that the spectral index evolves on very fast timescales (as short as 10 minutes), switching between optically thick and thin synchrotron emission, possibly due to instabilities in the compact jet or stochastic instabilities in the. accretion rate. We explore different scenarios to explain this very fast variability.
C1 [Rana, Vikram; Walton, Dominic J.; Fuerst, Felix; Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.; Tendulkar, Shriharsh] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Loh, Alan; Corbel, Stephane] Univ Paris Diderot, Lab AIM, CEA, IRFU,CNRS,INSU,DSM,SAp, F-91191 Gif Sur Yvette, France.
[Corbel, Stephane] Univ Orleans, Stn Radioastron Nancay, PSL Res Univ, Observ Paris,CNRS,OSUC, F-18330 Nancay, France.
[Tomsick, John A.; Boggs, Steven E.; Craig, William] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Barret, Didier] Univ Toulouse, UPS, OMP, IRAP, Toulouse, France.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Craig, William] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Gandhi, Poshak] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Hailey, Charles] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[Rahoui, Farid] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Rahoui, Farid] Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rana, V (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Madsen, Kristin/0000-0003-1252-4891;
Rana, Vikram/0000-0003-1703-8796
FU NASA [NNG08FD60C]; UnivEarthS Labex programme of Sorbonne Paris Cite
[ANR-10-LABX-0023, ANR-11-IDEX-0005-02]; CHAOS project - French Research
National Agency [ANR-12-BS05-0009]; NASA under XMM-Newton Guest Observer
grant [NNX14AF08G]; NuSTAR Operation, Software, and Calibration teams
FX We thank Michael A. Nowak for useful discussions on the synchrotron
model. This work was supported under NASA contract No. NNG08FD60C, and
made use of data from the NuSTAR mission, a project led by the
California Institute of Technology, managed by the Jet Propulsion
Laboratory, and funded by NASA. We thank the NuSTAR Operation, Software,
and Calibration teams for support with the execution and analysis of
these observations. This research has made use of the NuSTAR Data
Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data
Center (ASDC, Italy) and the California Institute of Technology (USA).
S.C. thanks James Miller-Jones for excellent help during the preparation
of the VLA observations. S.C. and A.L. acknowledge the financial support
from the UnivEarthS Labex programme of Sorbonne Paris Cite
(ANR-10-LABX-0023 and ANR-11-IDEX-0005-02), and from the CHAOS project
ANR-12-BS05-0009 supported by the French Research National Agency.
J.A.T. acknowledges partial support from NASA under XMM-Newton Guest
Observer grant NNX14AF08G.
NR 57
TC 7
Z9 7
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2016
VL 821
IS 2
AR 103
DI 10.3847/0004-637X/821/2/103
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DN5JM
UT WOS:000377102700032
ER
PT J
AU Sterling, AC
Moore, RL
Falconer, DA
Panesar, NK
Akiyama, S
Yashiro, S
Gopalswamy, N
AF Sterling, Alphonse C.
Moore, Ronald L.
Falconer, David A.
Panesar, Navdeep K.
Akiyama, Sachiko
Yashiro, Seiji
Gopalswamy, Nat
TI MINIFILAMENT ERUPTIONS THAT DRIVE CORONAL JETS IN A SOLAR ACTIVE REGION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: filaments, prominences; Sun: flares; Sun: magnetic
fields; Sun: UV radiation
ID X-RAY JETS; MAGNETIC-FIELD PROPERTIES; MASS EJECTIONS; FILAMENT
ERUPTIONS; BLOWOUT JET; FLUX ROPE; FLARES; DYNAMICS; RECONNECTION;
PROMINENCE
AB We present observations of eruptive events in an active region adjacent to an on-disk coronal hole on 2012 June 30, primarily using data from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA), SDO/Helioseismic and Magnetic Imager (HMI), and STEREO-B. One eruption is of a large-scale (similar to 100 '') filament that is typical of other eruptions, showing slow-rise onset followed by a faster-rise motion starting as flare emissions begin. It also shows an "EUV crinkle" emission pattern, resulting from magnetic reconnections between the exploding filament-carrying field and surrounding field. Many EUV jets, some of which are surges, sprays and/or X-ray jets, also occur in localized areas of the active region. We examine in detail two relatively energetic ones, accompanied by GOES M1 and C1 flares, and a weaker one without a GOES signature. All three jets resulted from small-scale (similar to 20 '') filament eruptions consistent with a slow rise followed by a fast rise occurring with flare-like jet-bright-point brightenings. The two more-energetic jets showed crinkle patters, but the third jet did not, perhaps due to its weakness. Thus all three jets were consistent with formation via erupting minifilaments, analogous to large-scale filament eruptions and to X-ray jets in polar coronal holes. Several other energetic jets occurred in a nearby portion of the active region; while their behavior was also consistent with their source being minifilament eruptions, we could not confirm this because their onsets were hidden from our view. Magnetic flux cancelation and emergence are candidates for having triggered the minifilament eruptions.
C1 [Sterling, Alphonse C.; Moore, Ronald L.; Falconer, David A.; Panesar, Navdeep K.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Moore, Ronald L.; Falconer, David A.; Panesar, Navdeep K.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Akiyama, Sachiko; Yashiro, Seiji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Akiyama, Sachiko; Yashiro, Seiji; Gopalswamy, Nat] Catholic Univ Amer, Washington, DC 20064 USA.
RP Sterling, AC (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM alphonse.sterling@nasa.gov; ron.moore@nasa.gov
OI Panesar, Navdeep/0000-0001-7620-362X
FU Heliophysics Division of NASA's Science Mission Directorate through
Living With a Star Targeted Research and Technology Program (LWS TRT);
Hinode project
FX We thank the anonymous referee for helpful comments. A.C.S., R.L.M.,
D.A.F., and N.K.P. were supported by funding from the Heliophysics
Division of NASA's Science Mission Directorate through the Living With a
Star Targeted Research and Technology Program (LWS TR&T), and the Hinode
project.
NR 58
TC 7
Z9 7
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2016
VL 821
IS 2
AR 100
DI 10.3847/0004-637X/821/2/100
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DN5JM
UT WOS:000377102700029
ER
PT J
AU Zucker, C
Walker, LM
Johnson, K
Gallagher, S
Alatalo, K
Tzanavaris, P
AF Zucker, Catherine
Walker, Lisa May
Johnson, Kelsey
Gallagher, Sarah
Alatalo, Katherine
Tzanavaris, Panayiotis
TI HIERARCHICAL FORMATION IN ACTION: CHARACTERIZING ACCELERATED GALAXY
EVOLUTION IN COMPACT GROUPS USING WHOLE-SKY WISE DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: groups: general; galaxies: interactions
ID INFRARED-EMISSION; AROMATIC FEATURES; STAR-CLUSTERS; GREEN VALLEY;
ULTRAVIOLET; HYPERLEDA; SPITZER; SAMPLE; ATLAS; SWIFT
AB Compact groups provide an environment to study the growth of galaxies amid multiple prolonged interactions. With their dense galaxy concentrations and relatively low velocity dispersions, compact groups mimic the conditions of hierarchical galaxy assembly. Compact group galaxies are known to show a bimodality in Spitzer IRAC infrared color space: galaxies are preferentially either quiescent with low specific star formation rates (SSFRs) or prolifically forming stars-galaxies with moderate levels of specific star formation are rare. Previous Spitzer IRAC studies identifying this "canyon" have been limited by small number statistics. We utilize whole-sky Wide-field Infrared Survey Explorer (WISE) data to study 163 compact groups, thereby tripling our previous sample and including more galaxies with intermediate mid-IR colors indicative of moderate SSFRs. We define a distinct WISE. mid-IR color space (log [f(12)/f(4.6)]) versus (log [f(22)/f(3.4)]) that we use to identify canyon galaxies from the larger sample. We confirm that compact group galaxies show a bimodal distribution in the mid-infrared and identify 37 canyon galaxies with reliable photometry and intermediate mid-IR colors. Morphologically, we find that the canyon harbors a large population of both Sa-Sbc and E/S0 type galaxies, and that they fall on the optical red sequence rather than the green valley. Finally, we provide a catalog of WISE. photometry for 567 of 652 galaxies selected from the sample of 163 compact groups.
C1 [Zucker, Catherine; Johnson, Kelsey] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Zucker, Catherine] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Walker, Lisa May] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Gallagher, Sarah] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Gallagher, Sarah] Univ Western Ontario, Ctr Planetary & Space Explorat, London, ON N6A 3K7, Canada.
[Alatalo, Katherine] Carnegie Observ, Pasadena, CA 91101 USA.
[Alatalo, Katherine] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Tzanavaris, Panayiotis] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Mail Code 662, Greenbelt, MD 20771 USA.
[Tzanavaris, Panayiotis] Univ Maryland Baltimore Cty, CRESST, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Tzanavaris, Panayiotis] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Zucker, C (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.; Zucker, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM catherine.zucker@cfa.harvard.edu
OI Zucker, Catherine/0000-0002-2250-730X; Alatalo,
Katherine/0000-0002-4261-2326
FU National Aeronautics and Space Administration; Alfred P. Sloan
Foundation; U.S. Department of Energy Office of Science; Virginia Space
Grant Consortium; University of Virginia College of Arts and Sciences;
Natural Sciences and Engineering Research Council of Canada
FX This publication makes use of data products from the Wide-field Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration.; Funding for the Sloan Digital Sky Survey IV has been
provided by the Alfred P. Sloan Foundation, the U.S. Department of
Energy Office of Science, and the Participating Institutions. SDSS-IV
acknowledges support and resources from the Center for High-Performance
Computing at the University of Utah. The SDSS Web site is www.sdss.org.;
C.S.Z. would like to sincerely thank the anonymous referee for their
thorough feedback throughout the review process. She would also like to
thank the Virginia Space Grant Consortium and the University of Virginia
College of Arts and Sciences for support.; S.C.G. thanks the Natural
Sciences and Engineering Research Council of Canada for support.
NR 32
TC 1
Z9 1
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2016
VL 821
IS 2
AR 113
DI 10.3847/0004-637X/821/2/113
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DN5JM
UT WOS:000377102700042
ER
PT J
AU Bernard, L
Blanchet, L
Bohe, A
Faye, G
Marsat, S
AF Bernard, Laura
Blanchet, Luc
Bohe, Alejandro
Faye, Guillaume
Marsat, Sylvain
TI Fokker action of nonspinning compact binaries at the fourth
post-Newtonian approximation
SO PHYSICAL REVIEW D
LA English
DT Article
ID GRAVITATIONAL-RADIATION REACTION; POINT-MASS SYSTEMS; MANY-BODY SYSTEM;
GENERAL-RELATIVITY; CANONICAL FORMALISM; 2-BODY PROBLEM; WAVE TAILS;
EQUATIONS; ORDER; MOTION
AB The Fokker action governing the motion of compact binary systems without spins is derived in harmonic coordinates at the fourth post-Newtonian approximation (4PN) of general relativity. Dimensional regularization is used for treating the local ultraviolet (UV) divergences associated with point particles, followed by a renormalization of the poles into a redefinition of the trajectories of the point masses. Effects at the 4PN order associated with wave tails propagating at infinity are included consistently at the level of the action. A finite part procedure based on analytic continuation deals with the infrared (IR) divergencies at spatial infinity, which are shown to be fully consistent with the presence of near-zone tails. Our end result at 4PN order is Lorentz invariant and has the correct self-force limit for the energy of circular orbits. However, we find that it differs from the recently published result derived within the ADM Hamiltonian formulation of general relativity [T. Damour, P. Jaranowski, and G. Schafer, Phys. Rev. D 89, 064058 (2014)]. More work is needed to understand this discrepancy.
C1 [Bernard, Laura; Blanchet, Luc; Faye, Guillaume] Sorbonne Univ, CNRS, UMR 7095, GReCO,Inst Astrophys Paris, 98Bis Blvd Arago, F-75014 Paris, France.
[Bernard, Laura; Blanchet, Luc; Faye, Guillaume] Univ Paris 06, 98Bis Blvd Arago, F-75014 Paris, France.
[Bohe, Alejandro] Albert Einstein Inst, Muehlenberg 1, D-14476 Potsdam, Germany.
[Marsat, Sylvain] Univ Maryland, Dept Phys, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA.
[Marsat, Sylvain] Univ Maryland, Joint Space Sci Ctr, College Pk, MD 20742 USA.
[Marsat, Sylvain] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
RP Bernard, L; Blanchet, L; Faye, G (reprint author), Sorbonne Univ, CNRS, UMR 7095, GReCO,Inst Astrophys Paris, 98Bis Blvd Arago, F-75014 Paris, France.; Bernard, L; Blanchet, L; Faye, G (reprint author), Univ Paris 06, 98Bis Blvd Arago, F-75014 Paris, France.; Bohe, A (reprint author), Albert Einstein Inst, Muehlenberg 1, D-14476 Potsdam, Germany.; Marsat, S (reprint author), Univ Maryland, Dept Phys, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA.; Marsat, S (reprint author), Univ Maryland, Joint Space Sci Ctr, College Pk, MD 20742 USA.; Marsat, S (reprint author), NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
EM bernard@iap.fr; blanchet@iap.fr; alejandro.bohe@aei.mpg.de; faye@iap.fr;
sylvain.marsat@aei.mpg.de
FU NASA [11-ATP-046, NNX12AN10G]
FX We are grateful to Thibault Damour for bringing to our attention, at an
early stage of this work, useful properties of the Fokker action, and
for informative comments regarding the DJS paper [67]. We also thank
Gilles Esposito-Farese and Gerhard Schafer for interesting discussions.
S. M. was supported by NASA Grant No. 11-ATP-046, as well as NASA Grant
No. NNX12AN10G at the University of Maryland College Park.
NR 92
TC 9
Z9 9
U1 1
U2 4
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD APR 20
PY 2016
VL 93
IS 8
AR 084037
DI 10.1103/PhysRevD.93.084037
PG 33
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DJ9RZ
UT WOS:000374551900010
ER
PT J
AU Ajello, M
Albert, A
Anderson, B
Baldini, L
Barbiellini, G
Bastieri, D
Bellazzini, R
Bissaldi, E
Blandford, RD
Bloom, ED
Bonino, R
Bottacini, E
Bregeon, J
Bruel, P
Buehler, R
Caliandro, GA
Cameron, RA
Caragiulo, M
Caraveo, PA
Cecchi, C
Chekhtman, A
Ciprini, S
Cohen-Tanugi, J
Conrad, J
Costanza, F
D'Ammando, F
de Angelis, A
de Palma, F
Desiante, R
Di Mauro, M
Di Venere, L
Dominguez, A
Drell, PS
Favuzzi, C
Focke, WB
Franckowiak, A
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Glanzman, T
Godfrey, G
Guiriec, S
Horan, D
Johannesson, G
Katsuragawa, M
Kensei, S
Kuss, M
Larsson, S
Latronico, L
Li, J
Li, L
Longo, F
Loparco, F
Lubrano, P
Madejski, GM
Maldera, S
Manfreda, A
Mayer, M
Mazziotta, MN
Meyer, M
Michelson, PF
Mirabal, N
Mizuno, T
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Negro, M
Nuss, E
Okada, C
Orlando, E
Ormes, JF
Paneque, D
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Sanchez-Conde, M
Sgro, C
Simone, D
Siskind, EJ
Spada, F
Spandre, G
Spinelli, P
Takahashi, H
Thayer, JB
Torres, DF
Tosti, G
Troja, E
Uchiyama, Y
Wood, KS
Wood, M
Zaharijas, G
Zimmer, S
AF Ajello, M.
Albert, A.
Anderson, B.
Baldini, L.
Barbiellini, G.
Bastieri, D.
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bloom, E. D.
Bonino, R.
Bottacini, E.
Bregeon, J.
Bruel, P.
Buehler, R.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Caraveo, P. A.
Cecchi, C.
Chekhtman, A.
Ciprini, S.
Cohen-Tanugi, J.
Conrad, J.
Costanza, F.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Desiante, R.
Di Mauro, M.
Di Venere, L.
Dominguez, A.
Drell, P. S.
Favuzzi, C.
Focke, W. B.
Franckowiak, A.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Glanzman, T.
Godfrey, G.
Guiriec, S.
Horan, D.
Johannesson, G.
Katsuragawa, M.
Kensei, S.
Kuss, M.
Larsson, S.
Latronico, L.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lubrano, P.
Madejski, G. M.
Maldera, S.
Manfreda, A.
Mayer, M.
Mazziotta, M. N.
Meyer, M.
Michelson, P. F.
Mirabal, N.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Negro, M.
Nuss, E.
Okada, C.
Orlando, E.
Ormes, J. F.
Paneque, D.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Sanchez-Conde, M.
Sgro, C.
Simone, D.
Siskind, E. J.
Spada, F.
Spandre, G.
Spinelli, P.
Takahashi, H.
Thayer, J. B.
Torres, D. F.
Tosti, G.
Troja, E.
Uchiyama, Y.
Wood, K. S.
Wood, M.
Zaharijas, G.
Zimmer, S.
CA Fermi-LAT Collaboration
TI Search for Spectral Irregularities due to Photon-Axionlike-Particle
Oscillations with the Fermi Large Area Telescope
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID EXTRAGALACTIC BACKGROUND LIGHT; GAMMA-RAY SPECTRA; MAGNETIC-FIELDS;
INVISIBLE AXION; PERSEUS CLUSTER; GALAXY CLUSTER; BLAZARS; CONSEQUENCES;
EVOLUTION; EMISSION
AB We report on the search for spectral irregularities induced by oscillations between photons and axionlike-particles (ALPs) in the gamma-ray spectrum of NGC 1275, the central galaxy of the Perseus cluster. Using 6 years of Fermi Large Area Telescope data, we find no evidence for ALPs and exclude couplings above 5 x 10(-12) GeV-1 for ALP masses 0.5 less than or similar to m(a) less than or similar to 5 neV at 95% confidence. The limits are competitive with the sensitivity of planned laboratory experiments, and, together with other bounds, strongly constrain the possibility that ALPs can reduce the gamma-ray opacity of the Universe.
C1 [Ajello, M.; Dominguez, A.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Albert, A.; Baldini, L.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Di Mauro, M.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Porter, T. A.; Reimer, A.; Thayer, J. B.; Wood, M.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Albert, A.; Baldini, L.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Di Mauro, M.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Porter, T. A.; Reimer, A.; Thayer, J. B.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Anderson, B.; Conrad, J.; Meyer, M.; Sanchez-Conde, M.; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Anderson, B.; Conrad, J.; Larsson, S.; Li, L.; Meyer, M.; Sanchez-Conde, M.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.; Bellazzini, R.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Longo, F.; Zaharijas, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bissaldi, E.; Caragiulo, M.; Costanza, F.; de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Simone, D.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bonino, R.; Desiante, R.; Latronico, L.; Maldera, S.; Negro, M.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bonino, R.; Negro, M.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34059 Montpellier, France.
[Bruel, P.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Buehler, R.; Mayer, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cecchi, C.; Ciprini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA.
[Ciprini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00133 Rome, Italy.
[D'Ammando, F.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy.
[de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Fukazawa, Y.; Kensei, S.; Okada, C.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Funk, S.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Guiriec, S.; Mirabal, N.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, Dunhaga 3, IS-107 Reykjavik, Iceland.
[Katsuragawa, M.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
[Larsson, S.; Li, L.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Li, J.; Torres, D. F.] IEEC CSIC, Inst Space Sci, Campus UAB, E-08193 Barcelona, Spain.
[Mizuno, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Murgia, S.] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Reimer, A.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Uchiyama, Y.] Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan.
[Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Zaharijas, G.] Univ Trieste, I-34127 Trieste, Italy.
[Zaharijas, G.] Univ Nova Gorica, Lab Astroparticle Phys, Vipavska 13, SI-5000 Nova Gorica, Slovenia.
RP Conrad, J; Meyer, M; Sanchez-Conde, M (reprint author), Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.; Conrad, J; Meyer, M; Sanchez-Conde, M (reprint author), AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
EM conrad@fysik.su.se; manuel.meyer@fysik.su.se; sanchezconde@fysik.su.se
RI Moskalenko, Igor/A-1301-2007; Bissaldi, Elisabetta/K-7911-2016; Meyer,
Manuel/E-2697-2016; Orlando, E/R-5594-2016; Funk, Stefan/B-7629-2015;
Bonino, Raffaella/S-2367-2016; Torres, Diego/O-9422-2016; Di Venere,
Leonardo/C-7619-2017;
OI Baldini, Luca/0000-0002-9785-7726; Moskalenko, Igor/0000-0001-6141-458X;
Bissaldi, Elisabetta/0000-0001-9935-8106; Meyer,
Manuel/0000-0002-0738-7581; Funk, Stefan/0000-0002-2012-0080; Torres,
Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X;
Sgro', Carmelo/0000-0001-5676-6214; Zaharijas,
Gabrijela/0000-0001-8484-7791; Pesce-Rollins,
Melissa/0000-0003-1790-8018; Mazziotta, Mario Nicola/0000-0001-9325-4672
FU Italian Ministry of Education, University and Research (MIUR)
[FIRB-2012-RBFR12PM1F]
FX The Fermi-LAT Collaboration acknowledges support for LAT development,
operation, and data analysis from NASA and DOE (U.S.), CEA/Irfu and
IN2P3/CNRS (France), ASI and INFN (Italy), MEXT, KEK, and JAXA (Japan),
and the K. A. Wallenberg Foundation, the Swedish Research Council, and
the National Space Board (Sweden). Science analysis support in the
operations phase from INAF (Italy) and CNES (France) is also gratefully
acknowledged. J. C. is a Wallenberg Academy Fellow. S. G. and N. M. are
NASA Postdoctoral Program Fellows. M. R. is funded by Contract No.
FIRB-2012-RBFR12PM1F from the Italian Ministry of Education, University
and Research (MIUR).
NR 75
TC 6
Z9 6
U1 2
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 20
PY 2016
VL 116
IS 16
AR 161101
DI 10.1103/PhysRevLett.116.161101
PG 7
WC Physics, Multidisciplinary
SC Physics
GA DJ9UU
UT WOS:000374559300002
PM 27152783
ER
PT J
AU Schwieterman, EW
Meadows, VS
Domagal-Goldman, SD
Deming, D
Arney, GN
Luger, R
Harman, CE
Misra, A
Barnes, R
AF Schwieterman, Edward W.
Meadows, Victoria S.
Domagal-Goldman, Shawn D.
Deming, Drake
Arney, Giada N.
Luger, Rodrigo
Harman, Chester E.
Misra, Amit
Barnes, Rory
TI IDENTIFYING PLANETARY BIOSIGNATURE IMPOSTORS: SPECTRAL FEATURES OF CO
AND O-4 RESULTING FROM ABIOTIC O-2/O-3 PRODUCTION (vol 819, pg L13,
2016)
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Correction
C1 [Schwieterman, Edward W.; Meadows, Victoria S.; Arney, Giada N.; Luger, Rodrigo; Misra, Amit; Barnes, Rory] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
[Schwieterman, Edward W.; Meadows, Victoria S.; Domagal-Goldman, Shawn D.; Deming, Drake; Arney, Giada N.; Luger, Rodrigo; Harman, Chester E.; Misra, Amit; Barnes, Rory] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA USA.
[Schwieterman, Edward W.; Meadows, Victoria S.; Arney, Giada N.; Luger, Rodrigo; Misra, Amit; Barnes, Rory] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA.
[Domagal-Goldman, Shawn D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Harman, Chester E.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Harman, Chester E.] Penn State Astrobiol Res Ctr, 2217 Earth & Engn Sci Bldg, University Pk, PA 16802 USA.
[Harman, Chester E.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
RP Schwieterman, EW (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM eschwiet@uw.edu
OI Schwieterman, Edward/0000-0002-2949-2163
NR 1
TC 1
Z9 1
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 20
PY 2016
VL 821
IS 2
AR L34
DI 10.3847/2041-8205/821/2/L34
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6OD
UT WOS:000374331900015
ER
PT J
AU Bergano, M
Rocha, A
Cupido, L
Barbosa, D
Villela, T
Boas, JV
Rocha, G
Smoot, GF
AF Bergano, Miguel
Rocha, Armando
Cupido, Luis
Barbosa, Domingos
Villela, Thyrso
Boas, Jose Vilas
Rocha, Graca
Smoot, George F.
TI A high performance cost-effective digital complex correlator for an
X-band polarimetry survey
SO SPRINGERPLUS
LA English
DT Article
DE Radioastronomy (astronomy, astrophysics and cosmology); Logic design
(hardware); Register-transfer-level implementation (hardware)
ID POLARIZATION; EMISSION
AB The detailed knowledge of the Milky Way radio emission is important to characterize galactic foregrounds masking extragalactic and cosmological signals. The update of the global sky models describing radio emissions over a very large spectral band requires high sensitivity experiments capable of observing large sky areas with long integration times. Here, we present the design of a new 10 GHz (X-band) polarimeter digital back-end to map the polarization components of the galactic synchrotron radiation field of the Northern Hemisphere sky. The design follows the digital processing trends in radio astronomy and implements a large bandwidth (1 GHz) digital complex cross-correlator to extract the Stokes parameters of the incoming synchrotron radiation field. The hardware constraints cover the implemented VLSI hardware description language code and the preliminary results. The implementation is based on the simultaneous digitized acquisition of the Cartesian components of the two linear receiver polarization channels. The design strategy involves a double data rate acquisition of the ADC interleaved parallel bus, and field programmable gate array device programming at the register transfer mode. The digital core of the back-end is capable of processing 32 Gbps and is built around an Altera field programmable gate array clocked at 250 MHz, 1 GSps analog to digital converters and a clock generator. The control of the field programmable gate array internal signal delays and a convenient use of its phase locked loops provide the timing requirements to achieve the target bandwidths and sensitivity. This solution is convenient for radio astronomy experiments requiring large bandwidth, high functionality, high volume availability and low cost. Of particular interest, this correlator was developed for the Galactic Emission Mapping project and is suitable for large sky area polarization continuum surveys. The solutions may also be adapted to be used at signal processing subsystem levels for large projects like the square kilometer array testbeds.
C1 [Bergano, Miguel] Univ Aveiro, Inst Telecomunicacoes, DETI, Campus Univ Santiago, P-3810193 Aveiro, Portugal.
[Rocha, Armando] Univ Aveiro, DETI, Campus Univ Santiago, P-3810106 Aveiro, Portugal.
[Cupido, Luis] LC Technol, Aveiro, Portugal.
[Barbosa, Domingos] Inst Telecomunicacoes, Campus Univ Santiago, P-3810193 Aveiro, Portugal.
[Villela, Thyrso; Boas, Jose Vilas] INPE, Div Astrofis DAS, Ave Astronautas 1-758, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Rocha, Graca] CALTECH, Jet Prop Lab, M-S 169-327,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Rocha, Graca] CALTECH, Cahill Bldg MS 59-33 1200 E Calif, Pasadena, CA 91125 USA.
[Smoot, George F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, 1 Cyclotron Rd,MS 50-5005, Berkeley, CA 94720 USA.
[Smoot, George F.] Univ Paris Diderot APC, Batiment Condorcet, F-75205 Paris 13, France.
RP Bergano, M (reprint author), Univ Aveiro, Inst Telecomunicacoes, DETI, Campus Univ Santiago, P-3810193 Aveiro, Portugal.
EM jbergano@av.it.pt
FU Fundacao para a Ciencia e a Tecnologia (FCT) the Portuguese national
funding agency [SFRH/BD/76615/2011]; FCT/MEC through national funds;
FEDER-PT2020 [UID/EEA/50008/2013]
FX The corresponding author acknowledge support from the Fundacao para a
Ciencia e a Tecnologia (FCT) the Portuguese national funding agency
(SFRH/BD/76615/2011) and by FCT/MEC through national funds and when
applicable co-funded by FEDER-PT2020 partnership agreement under the
project UID/EEA/50008/2013.
NR 25
TC 0
Z9 0
U1 2
U2 2
PU SPRINGER INTERNATIONAL PUBLISHING AG
PI CHAM
PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND
SN 2193-1801
J9 SPRINGERPLUS
JI SpringerPlus
PD APR 19
PY 2016
VL 5
AR 487
DI 10.1186/s40064-016-2109-5
PG 14
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DL5UB
UT WOS:000375701400008
PM 27218002
ER
PT J
AU Nadeau, JL
Bin Cho, Y
Kuhn, J
Liewer, K
AF Nadeau, Jay L.
Bin Cho, Yong
Kuhn, Jonas
Liewer, Kurt
TI Improved Tracking and Resolution of Bacteria in Holographic Microscopy
Using Dye and Fluorescent Protein Labeling
SO FRONTIERS IN CHEMISTRY
LA English
DT Article
DE digital holographic microscopy; interferometric microscopy; quantitative
phase imaging; bacterial tracking; bacterial motility; green fluorescent
proteins; Mach-Zehnder
ID INTRINSIC SPECKLE NOISE; PHASE-CONTRAST; PARTICLE HOLOGRAPHY;
REFRACTIVE-INDEX; LIVING CELLS; 3D; COMPENSATION; REFLECTION
AB Digital holographic microscopy (DHM) is an emerging imaging technique that permits instantaneous capture of a relatively large sample volume. However, large volumes usually come at the expense of lower spatial resolution, and the technique has rarely been used with prokaryotic cells due to their small size and low contrast. In this paper we demonstrate the use of a Mach-Zehnder dual-beam instrument for imaging of labeled and unlabeled bacteria and microalgae. Spatial resolution of 0.3 mu m is achieved, providing a sampling of several pixels across a typical prokaryotic cell. Both cellular motility and morphology are readily recorded. The use of dyes provides both amplitude and phase contrast improvement and is of use to identify cells in dense samples.
C1 [Nadeau, Jay L.; Bin Cho, Yong; Kuhn, Jonas] CALTECH, Grad Aeronaut Labs, Pasadena, CA 91125 USA.
[Nadeau, Jay L.; Bin Cho, Yong] McGill Univ, Dept Biomed Engn, Montreal, PQ, Canada.
[Kuhn, Jonas] ETH, Inst Astron, CH-8092 Zurich, Switzerland.
[Liewer, Kurt] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Nadeau, JL (reprint author), CALTECH, Grad Aeronaut Labs, Pasadena, CA 91125 USA.; Nadeau, JL (reprint author), McGill Univ, Dept Biomed Engn, Montreal, PQ, Canada.
EM jnadeau@caltech.edu
FU Gordon and Betty Moore Foundation (GBMF) [4037, 4038]
FX This work was supported by the Gordon and Betty Moore Foundation (GBMF)
grant numbers 4037 (McGill University) and 4038 (California Institute of
Technology). We also thank the Keck Institute for Space Studies for
allowing us use of the Tolman/Bacher House, which served as a meeting
location for our team on the Caltech campus. We appreciate the
contribution of Asphericon, Inc. for fabricating customized optical
elements to meet the packaging needs. This work was partially carried
out by the Jet Propulsion Laboratory, California Institute of
Technology.
NR 37
TC 0
Z9 0
U1 13
U2 13
PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
EI 2296-2646
J9 FRONT CHEM
JI Front. Chem.
PD APR 19
PY 2016
VL 4
AR 17
DI 10.3389/fchem.2016.00017
PG 10
WC Chemistry, Multidisciplinary
SC Chemistry
GA DJ5WX
UT WOS:000374282600002
PM 27242995
ER
PT J
AU Peng, JF
Hu, M
Guo, S
Du, ZF
Zheng, J
Shang, DJ
Zamora, ML
Zeng, LM
Shao, M
Wu, YS
Zheng, J
Wang, Y
Glen, CR
Collins, DR
Molina, MJ
Zhang, RY
AF Peng, Jianfei
Hu, Min
Guo, Song
Du, Zhuofei
Zheng, Jing
Shang, Dongjie
Zamora, Misti Levy
Zeng, Limin
Shao, Min
Wu, Yu-Sheng
Zheng, Jun
Wang, Yuan
Glen, Crystal R.
Collins, Donald R.
Molina, Mario J.
Zhang, Renyi
TI Markedly enhanced absorption and direct radiative forcing of black
carbon under polluted urban environments
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE black carbon; absorption; air quality; radiative forcing; climate
ID OH-INITIATED OXIDATION; LIGHT-ABSORPTION; SOOT AEROSOLS; MIXING STATE;
AMPLIFICATION; PARTICLES; CONSISTENCY; RADICALS; IMPACTS; TOLUENE
AB Black carbon (BC) exerts profound impacts on air quality and climate because of its high absorption cross-section over a broad range of electromagnetic spectra, but the current results on absorption enhancement of BC particles during atmospheric aging remain conflicting. Here, we quantified the aging and variation in the optical properties of BC particles under ambient conditions in Beijing, China, and Houston, United States, using a novel environmental chamber approach. BC aging exhibits two distinct stages, i.e., initial transformation from a fractal to spherical morphology with little absorption variation and subsequent growth of fully compact particles with a large absorption enhancement. The timescales to achieve complete morphology modification and an absorption amplification factor of 2.4 for BC particles are estimated to be 2.3 h and 4.6 h, respectively, in Beijing, compared with 9 h and 18 h, respectively, in Houston. Our findings indicate that BC under polluted urban environments could play an essential role in pollution development and contribute importantly to large positive radiative forcing. The variation in direct radiative forcing is dependent on the rate and timescale of BC aging, with a clear distinction between urban cities in developed and developing countries, i.e., a higher climatic impact inmore polluted environments. We suggest that mediation in BC emissions achieves a cobenefit in simultaneously controlling air pollution and protecting climate, especially for developing countries.
C1 [Peng, Jianfei; Hu, Min; Guo, Song; Du, Zhuofei; Zheng, Jing; Shang, Dongjie; Zeng, Limin; Wu, Yu-Sheng; Zhang, Renyi] Peking Univ, State Key Joint Lab Environm Simulat & Pollut Con, Coll Environm Sci & Engn, Beijing 100871, Peoples R China.
[Guo, Song; Zamora, Misti Levy; Shao, Min; Zheng, Jun; Glen, Crystal R.; Collins, Donald R.; Zhang, Renyi] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Wang, Yuan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Molina, Mario J.] Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA.
[Zheng, Jun] Nanjing Univ Informat Sci & Technol, Jiangsu Key Lab Atmospher Environm Monitoring & P, Nanjing 210044, Jiangsu, Peoples R China.
[Glen, Crystal R.] Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA.
RP Hu, M; Zhang, RY (reprint author), Peking Univ, State Key Joint Lab Environm Simulat & Pollut Con, Coll Environm Sci & Engn, Beijing 100871, Peoples R China.; Zhang, RY (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.; Molina, MJ (reprint author), Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA.
EM minhu@pku.edu.cn; mjmolina@ucsd.edu; renyi-zhang@tamu.edu
RI Guo, Song/D-9218-2012; Zeng, Limin/D-3948-2013; Collins,
Don/F-9617-2012; Zhang, Renyi/A-2942-2011; Zheng, Jun/E-6772-2010; Peng,
Jianfei/F-1438-2015
OI Guo, Song/0000-0002-9661-2313;
FU National Natural Science Foundation of China [91544214, 21190052];
National Basic Research Program; China Ministry of Science and
Technology [2013CB228503]; China Ministry of Environmental Protection's
Special Funds for Scientific Research on Public Welfare [20130916];
Robert A. Welch Foundation [A-1417]; Houston Advanced Research Center
FX We thank Wei Hu and Zhaoheng Gong for their assistance with the AMS data
analysis, Wentai Chen and Yue Li for providing VOCs data, and Nan Ma for
providing the core-shell code for the Mie calculation. This work was
supported by National Natural Science Foundation of China (Grants
91544214 and 21190052), the National Basic Research Program, China
Ministry of Science and Technology (Grant 2013CB228503), National
Natural Science Foundation of China (Grant 21190052), and the China
Ministry of Environmental Protection's Special Funds for Scientific
Research on Public Welfare (Grant 20130916). R.Z. acknowledges support
from the Robert A. Welch Foundation (Grant A-1417) and Houston Advanced
Research Center.
NR 42
TC 31
Z9 32
U1 56
U2 93
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD APR 19
PY 2016
VL 113
IS 16
BP 4266
EP 4271
DI 10.1073/pnas.1602310113
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DJ7LV
UT WOS:000374393800030
PM 27035993
ER
PT J
AU Lavraud, B
Zhang, YC
Vernisse, Y
Gershman, DJ
Dorelli, J
Cassak, PA
Dargent, J
Pollock, C
Giles, B
Aunai, N
Argall, M
Avanov, L
Barrie, A
Burch, J
Chandler, M
Chen, LJ
Clark, G
Cohen, I
Coffey, V
Eastwood, JP
Egedal, J
Eriksson, S
Ergun, R
Farrugia, CJ
Fuselier, SA
Genot, V
Graham, D
Grigorenko, E
Hasegawa, H
Jacquey, C
Kacem, I
Khotyaintsev, Y
MacDonald, E
Magnes, W
Marchaudon, A
Mauk, B
Moore, TE
Mukai, T
Nakamura, R
Paterson, W
Penou, E
Phan, TD
Rager, A
Retino, A
Rong, ZJ
Russell, CT
Saito, Y
Sauvaud, JA
Schwartz, SJ
Shen, C
Smith, S
Strangeway, R
Toledo-Redondo, S
Torbert, R
Turner, DL
Wang, S
Yokota, S
AF Lavraud, B.
Zhang, Y. C.
Vernisse, Y.
Gershman, D. J.
Dorelli, J.
Cassak, P. A.
Dargent, J.
Pollock, C.
Giles, B.
Aunai, N.
Argall, M.
Avanov, L.
Barrie, A.
Burch, J.
Chandler, M.
Chen, L. -J.
Clark, G.
Cohen, I.
Coffey, V.
Eastwood, J. P.
Egedal, J.
Eriksson, S.
Ergun, R.
Farrugia, C. J.
Fuselier, S. A.
Genot, V.
Graham, D.
Grigorenko, E.
Hasegawa, H.
Jacquey, C.
Kacem, I.
Khotyaintsev, Y.
MacDonald, E.
Magnes, W.
Marchaudon, A.
Mauk, B.
Moore, T. E.
Mukai, T.
Nakamura, R.
Paterson, W.
Penou, E.
Phan, T. D.
Rager, A.
Retino, A.
Rong, Z. J.
Russell, C. T.
Saito, Y.
Sauvaud, J. -A.
Schwartz, S. J.
Shen, C.
Smith, S.
Strangeway, R.
Toledo-Redondo, S.
Torbert, R.
Turner, D. L.
Wang, S.
Yokota, S.
TI Currents and associated electron scattering and bouncing near the
diffusion region at Earth's magnetopause
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MAGNETIC RECONNECTION; CURRENT SHEET; MAGNETOTAIL; CLUSTER; FIELD
AB Based on high-resolution measurements from NASA's Magnetospheric Multiscale mission, we present the dynamics of electrons associated with current systems observed near the diffusion region of magnetic reconnection at Earth's magnetopause. Using pitch angle distributions (PAD) and magnetic curvature analysis, we demonstrate the occurrence of electron scattering in the curved magnetic field of the diffusion region down to energies of 20 eV. We show that scattering occurs closer to the current sheet as the electron energy decreases. The scattering of inflowing electrons, associated with field-aligned electrostatic potentials and Hall currents, produces a new population of scattered electrons with broader PAD which bounce back and forth in the exhaust. Except at the center of the diffusion region the two populations are collocated and appear to behave adiabatically: the inflowing electron PAD focuses inward (toward lower magnetic field), while the bouncing population PAD gradually peaks at 90 degrees away from the center (where it mirrors owing to higher magnetic field and probable field-aligned potentials).
C1 [Lavraud, B.; Zhang, Y. C.; Vernisse, Y.; Dargent, J.; Genot, V.; Jacquey, C.; Kacem, I.; Marchaudon, A.; Penou, E.; Sauvaud, J. -A.] Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse, France.
[Lavraud, B.; Zhang, Y. C.; Vernisse, Y.; Dargent, J.; Genot, V.; Jacquey, C.; Kacem, I.; Marchaudon, A.; Penou, E.; Sauvaud, J. -A.] CNRS, UMR 5277, Toulouse, France.
[Zhang, Y. C.] CAS, NSSC, State Key Lab Space Weather, Beijing, Peoples R China.
[Gershman, D. J.; Dorelli, J.; Pollock, C.; Giles, B.; Avanov, L.; Barrie, A.; Chen, L. -J.; MacDonald, E.; Moore, T. E.; Paterson, W.; Rager, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Gershman, D. J.; Avanov, L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Cassak, P. A.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
[Dargent, J.; Aunai, N.; Retino, A.] Plasma Phys Lab, Palaiseau, France.
[Argall, M.; Farrugia, C. J.; Torbert, R.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Barrie, A.; Wang, S.] Millenium Engn & Integrat Co, Arlington, VA USA.
[Burch, J.; Fuselier, S. A.] SW Res Inst, San Antonio, TX USA.
[Chandler, M.; Coffey, V.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA.
[Clark, G.; Cohen, I.; Mauk, B.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Eastwood, J. P.; Schwartz, S. J.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London, England.
[Egedal, J.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
[Eriksson, S.; Ergun, R.; Schwartz, S. J.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Graham, D.; Khotyaintsev, Y.] Swedish Inst Space Phys, Uppsala, Sweden.
[Grigorenko, E.] Russian Acad Sci, Space Res Inst, Moscow, Russia.
[Hasegawa, H.; Mukai, T.; Saito, Y.; Yokota, S.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa, Japan.
[Magnes, W.; Nakamura, R.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
[Phan, T. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Rager, A.; Smith, S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Rong, Z. J.] CAS, IGG, Key Lab Earth & Planetary Phys, Beijing, Peoples R China.
[Russell, C. T.; Strangeway, R.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Shen, C.] Harbin Inst Technol, Shenzhen, Peoples R China.
[Toledo-Redondo, S.] ESAC ESA, Villafranca Del Castillo, Spain.
[Turner, D. L.] Aerosp Corp, El Segundo, CA 90245 USA.
RP Lavraud, B (reprint author), Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse, France.; Lavraud, B (reprint author), CNRS, UMR 5277, Toulouse, France.
EM Benoit.Lavraud@irap.omp.eu
RI Hasegawa, Hiroshi/A-1192-2007; Nakamura, Rumi/I-7712-2013; Cohen,
Ian/K-3038-2015; NASA MMS, Science Team/J-5393-2013; Mauk,
Barry/E-8420-2017;
OI Zhang, Yongcun/0000-0001-5721-8164; Hasegawa,
Hiroshi/0000-0002-1172-021X; Nakamura, Rumi/0000-0002-2620-9211; Cohen,
Ian/0000-0002-9163-6009; NASA MMS, Science Team/0000-0002-9504-5214;
Mauk, Barry/0000-0001-9789-3797; Eriksson, Stefan/0000-0002-5619-1577
FU CNRS; CNES; Leverhulme Trust
FX For MMS data, visit https://lasp.colorado.edu/mms/sdc/public/. We thank
all the MMS teams for their remarkable work and great hardware
accomplishments. Work at IRAP was performed with the support of CNRS and
CNES. The authors would like to thank the SMILEI development team for
their support and providing them with the code SMILEI. S.J.S. thanks the
Leverhulme Trust for its award of a Research Fellowship.
NR 39
TC 14
Z9 14
U1 4
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2016
VL 43
IS 7
BP 3042
EP 3050
DI 10.1002/2016GL068359
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DL3MG
UT WOS:000375537300005
ER
PT J
AU Maldonado, AA
Chen, LJ
Claudepierre, SG
Bortnik, J
Thorne, RM
Spence, H
AF Maldonado, Armando A.
Chen, Lunjin
Claudepierre, Seth G.
Bortnik, Jacob
Thorne, Richard M.
Spence, Harlan
TI Electron butterfly distribution modulation by magnetosonic waves
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID RELATIVISTIC ELECTRONS; MAGNETIC-FIELD; SCATTERING; PARTICLE
AB The butterfly pitch angle distribution is observed as a dip in an otherwise normal distribution of electrons centered about alpha(eq) = 90 degrees. During storm times, the formation of the butterfly distribution on the nightside magnetosphere has been attributed to L shell splitting combined with magnetopause shadowing and strong positive radial flux gradients. It has been shown that this distribution can be caused by combined chorus and magnetosonic wave scattering where the two waves work together but at different local times. Presented in our study is an event on 21 August 2013, using Van Allen Probe measurements, where a butterfly distribution formation is modulated by local magnetosonic coherent magnetosonic waves intensity. Transition from normal to butterfly distributions coincides with rising magnetosonic wave intensity while an opposite transition occurs when wave intensity diminishes. We propose that bounce resonance with waves is the underlying process responsible for such rapid modulation, which is confirmed by our test particle simulation.
C1 [Maldonado, Armando A.; Chen, Lunjin] Univ Texas Dallas, Dept Phys, Richardson, TX 75083 USA.
[Claudepierre, Seth G.] Aerosp Corp, Dept Space Sci, El Segundo, CA 90245 USA.
[Bortnik, Jacob; Thorne, Richard M.] Univ Calif Los Angeles, Atmospher & Ocean Sci Dept, Los Angeles, CA USA.
[Spence, Harlan] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Maldonado, AA (reprint author), Univ Texas Dallas, Dept Phys, Richardson, TX 75083 USA.
EM aam131130@utdallas.edu
FU NSF's Geospace Environment Modeling grant [AGS1405041, AGS-1103064];
NASA's grant [NNX15AF55G]; JHU/APL [967399, NAS5-01072]; NASA-LWS
[NNX13AI61G]
FX MagEIS data were provided by the Aerospace Corporation. EMFISIS data
were provided by NASA through spdf.gsfc.nasa.gov. We also acknowledge
the use of OMNI data. This work was supported by NSF's Geospace
Environment Modeling grant AGS1405041 and NASA's grant NNX15AF55G,
NASA-LWS grant NNX13AI61G, and RBSP-ECT funding is provided by JHU/APL
contract 967399 under NASA's Prime contract NAS5-01072. J.B. would like
to gratefully acknowledge the support of NSF's Geospace Environment
Modeling grant AGS-1103064.
NR 23
TC 3
Z9 3
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2016
VL 43
IS 7
BP 3051
EP 3059
DI 10.1002/2016GL068161
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DL3MG
UT WOS:000375537300006
ER
PT J
AU Landis, ME
Byrne, S
Daubar, IJ
Herkenhoff, KE
Dundas, CM
AF Landis, Margaret E.
Byrne, Shane
Daubar, Ingrid J.
Herkenhoff, Kenneth E.
Dundas, Colin M.
TI A revised surface age for the North Polar Layered Deposits of Mars
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID CRATERING RATE; IMPACT CRATERS; CAP; STRATIGRAPHY; CLIMATE; RATES;
EVOLUTION; EVENTS; SIZE; FLOW
AB The North Polar Layered Deposits (NPLD) of Mars contain a complex stratigraphy that has been suggested to retain a record of past eccentricity- and obliquity-forced climate changes. The surface accumulation rate in the current climate can be constrained by the crater retention age. We scale NPLD crater diameters to account for icy target strength and compare surface age using a new production function for recent small impacts on Mars to the previously used model of Hartmann (2005). Our results indicate that ice is accumulating in these craters several times faster than previously thought, with a 100m diameter crater being completely infilled within centuries. Craters appear to have a diameter-dependent lifetime, but the data also permit a complete resurfacing of the NPLD at similar to 1.5 ka.
C1 [Landis, Margaret E.; Byrne, Shane] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Daubar, Ingrid J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Herkenhoff, Kenneth E.; Dundas, Colin M.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
RP Landis, ME (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM mlandis@lpl.arizona.edu
OI Dundas, Colin/0000-0003-2343-7224
FU NASA [NNX13AG72G]; National Science Foundation Graduate Research
Fellowship Program [DGE-1143953]
FX This work was funded by NASA grant NNX13AG72G. M.E.L. was supported by
the National Science Foundation Graduate Research Fellowship Program,
grant DGE-1143953. HiRISE images referenced are available on the
instrument's public website: https://hirise.lpl.arizona.edu. The crater
catalog used in this work is included with this paper as supporting
information. The authors thank S. Sutton for help with SOCET Set
software, M.M. Sori for useful discussion on viscous relaxation, and
M.E. Banks for useful discussion on the impact population. The authors
additionally thank J.A. Skinner, P. Becerra, D. Laikko, M. Sori, N.
Barlow, and an anonymous reviewer for helpful comments on the
manuscript.
NR 43
TC 2
Z9 2
U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2016
VL 43
IS 7
BP 3060
EP 3068
DI 10.1002/2016GL068434
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DL3MG
UT WOS:000375537300007
ER
PT J
AU Poppe, AR
Halekas, JS
Szalay, JR
Horanyi, M
Levin, Z
Kempf, S
AF Poppe, A. R.
Halekas, J. S.
Szalay, J. R.
Horanyi, M.
Levin, Z.
Kempf, S.
TI LADEE/LDEX observations of lunar pickup ion distribution and variability
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ENVIRONMENT EXPLORER MISSION; PHOTON-STIMULATED DESORPTION; NEUTRAL
MASS-SPECTROMETER; SURFACE-COMPOSITION; DUST EXPERIMENT; ATMOSPHERE;
EXOSPHERE; SOLAR; LUTETIA; TARGETS
AB We report fortuitous observations of low-energy lunar pickup ion fluxes near the Moon while in the solar wind by the Lunar Dust Experiment (LDEX) on board the Lunar Atmosphere and Dust Environment Explorer (LADEE). We describe the method of observation and the empirical calibration of the instrument for ion observations. LDEX observes several trends in the exospheric ion production rate, including a scale height of approximately 100 km, a positive, linear correlation with solar wind flux, and evidence of a slight enhancement near 7-8 h local time. We compare the LDEX observations to both LADEE Neutral Mass Spectrometer ion mode observations and theoretical models. The LDEX data are best fit by total exospheric ion production rates of approximate to 6 x 10(3) m(-3) s(-1) with dominant contributions from Al+, CO+, and Ar+, although the LDEX data suggest that the aluminum neutral density and corresponding ion production rate are lower than predicted by recent models.
C1 [Poppe, A. R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Poppe, A. R.; Halekas, J. S.; Horanyi, M.; Kempf, S.] NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA.
[Halekas, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Szalay, J. R.] Southwest Res Inst, San Antonio, TX USA.
[Horanyi, M.; Levin, Z.; Kempf, S.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Horanyi, M.; Levin, Z.; Kempf, S.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
RP Poppe, AR (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.; Poppe, AR (reprint author), NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA.
EM poppe@ssl.berkeley.edu
FU NASA LADEE Guest Investigator program [NNX13AO71G]; NASA LASER program
[NNX13AJ97G]; NASA [NAS5-02099]; German Ministry for Economy and
Technology; German Center for Aviation and Space (DLR) [50-OC-0302]
FX A.R.P. and J.S.H. gratefully acknowledge support from both the NASA
LADEE Guest Investigator program, grant #NNX13AO71G, and the NASA LASER
program, grant #NNX13AJ97G. J.S., M.H., Z.L., and S.K. acknowledge
support from the NASA's SSERVI IMPACT team. The authors also thank R.C.
Elphic and G.T. Delory for their excellent work in leading the LADEE
team and ensuring the success of the mission. The ARTEMIS mission is
funded and operated under NASA grant #NAS5-02099, and we specifically
acknowledge J.P. McFadden for the use of ESA data and K.-H. Glassmeier,
U. Auster, and W. Baumjohann for the use of FGM data provided under the
lead of the Technical University of Braunschweig and with financial
support through the German Ministry for Economy and Technology and the
German Center for Aviation and Space (DLR) under contract 50-OC-0302.
ARTEMIS data are publicly available at http://artemis.ssl.berkeley.edu,
and LADEE/LDEX data are available through NASA's Planetary Data System.
Finally, the authors thank two reviewers for constructive comments.
NR 45
TC 2
Z9 2
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2016
VL 43
IS 7
BP 3069
EP 3077
DI 10.1002/2016GL068393
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DL3MG
UT WOS:000375537300008
ER
PT J
AU Anderson, CM
Samuelson, RE
Yung, YL
McLain, JL
AF Anderson, C. M.
Samuelson, R. E.
Yung, Y. L.
McLain, J. L.
TI Solid-state photochemistry as a formation mechanism for Titan's
stratospheric C4N2 ice clouds
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID NORTH POLAR STRATOSPHERE; DICYANOACETYLENE; ATMOSPHERE; CYANOACETYLENE;
CASSINI/CIRS; CONDENSATION; CHEMISTRY; SPECTRA
AB We propose that C4N2 ice clouds observed in Titan's springtime polar stratosphere arise due to solid-state photochemistry occurring within extant ice cloud particles of HCN-HC3N mixtures. This formation process resembles the halogen-induced ice particle surface chemistry that leads to condensed nitric acid trihydrate (NAT) particles and ozone depletion in Earth's polar stratosphere. As our analysis of the Cassini Composite Infrared Spectrometer 478 cm(-1) ice emission feature demonstrates, this solid-state photochemistry mechanism eliminates the need for the relatively high C4N2 saturation vapor pressures required (even though they are not observed) when the ice is produced through the usual procedure of direct condensation from the vapor.
C1 [Anderson, C. M.; Samuelson, R. E.; McLain, J. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Samuelson, R. E.; McLain, J. L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Yung, Y. L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Anderson, CM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM carrie.m.anderson@nasa.gov
FU NASA's Cassini Project; Cassini Data Analysis and Participating
Scientist program; Cassini UVIS program via NASA [JPL.1459109]
FX The authors acknowledge funding support from NASA's Cassini Project.
C.M.A. and R.E.S. were supported in part by the Cassini Data Analysis
and Participating Scientist program. Y.L.Y. was supported in part by the
Cassini UVIS program via NASA grant JPL.1459109 to the California
Institute of Technology. The CIRS data presented here are archived in
the PDS Atmospheres Node at New Mexico State University.
NR 29
TC 1
Z9 1
U1 5
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2016
VL 43
IS 7
BP 3088
EP 3094
DI 10.1002/2016GL067795
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DL3MG
UT WOS:000375537300010
ER
PT J
AU Han, SC
Sauber, J
Pollitz, F
AF Han, Shin-Chan
Sauber, Jeanne
Pollitz, Fred
TI Postseismic gravity change after the 2006-2007 great earthquake doublet
and constraints on the asthenosphere structure in the central Kuril
Islands
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SUMATRA-ANDAMAN EARTHQUAKE; TOHOKU-OKI EARTHQUAKE; VISCOELASTIC
RELAXATION; OCEAN CONTRIBUTION; SUBDUCTION ZONES; DEFORMATION; MODELS;
SYSTEM; SLAB; FLOW
AB Large earthquakes often trigger viscoelastic adjustment for years to decades depending on the rheological properties and the nature and spatial extent of coseismic stress. The 2006 M(w)8.3 thrust and 2007 M(w)8.1 normal fault earthquakes of the central Kuril Islands resulted in significant postseismic gravity change in Gravity Recovery and Climate Experiment (GRACE) but without a discernible coseismic gravity change. The gravity increase of similar to 4 mu Gal, observed consistently from various GRACE solutions around the epicentral area during 2007-2015, is interpreted as resulting from gradual seafloor uplift by similar to 6 cm produced by postseismic relaxation. The GRACE data are best fit with a model of 25-35 km for the elastic thickness and similar to 10(18) Pa s for the Maxwell viscosity of the asthenosphere. The large measurable postseismic gravity change (greater than coseismic change) emphasizes the importance of viscoelastic relaxation in understanding tectonic deformation and fault-locking scenarios in the Kuril subduction zone.
C1 [Han, Shin-Chan] Univ Newcastle, Sch Engn, Callaghan, NSW 2308, Australia.
[Sauber, Jeanne] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD USA.
[Pollitz, Fred] US Geol Survey, 345 Middlefield Rd, Menlo Pk, CA 94025 USA.
RP Han, SC (reprint author), Univ Newcastle, Sch Engn, Callaghan, NSW 2308, Australia.
EM shin-chan.han@newcastle.edu.au
FU NASA's GRACE project; Earth Surface and Interior program
FX This work was supported partly by NASA's GRACE project and Earth Surface
and Interior program. We thank Riccardo Riva for the computer codes of
the normal mode analysis used in Figure 3. We thank DLR for the GRACE
telemetry data and JPL, CSR, GFZ, and GRGS for the high-quality level 1B
and level 2 products. The GRACE data for this paper are available at
podaac.jpl.nasa.gov/GRACE and www.thegrace-plotter.com. We thank Jeanne
Hardebeck and Ruth Harris for their comments on a preliminary draft. We
thank Taco Broerse, an anonymous reviewer, and the Editor for their
constructive reviews.
NR 32
TC 2
Z9 2
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2016
VL 43
IS 7
BP 3169
EP 3177
DI 10.1002/2016GL068167
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DL3MG
UT WOS:000375537300020
PM 27642200
ER
PT J
AU Sabaka, TJ
Tyler, RH
Olsen, N
AF Sabaka, Terence J.
Tyler, Robert H.
Olsen, Nils
TI Extracting ocean-generated tidalmagnetic signals from Swarm data through
satellite gradiometry
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GEOMAGNETIC-FIELD MODEL; EARTHS MAGNETIC-FIELD; OBSERVATORY DATA;
CONDUCTIVITY; CONSTELLATION; MANTLE; CHAMP; TIME; YR
AB Ocean-generated magnetic field models of the Principal Lunar, M-2, and the Larger Lunar elliptic, N-2, semidiurnal tidal constituents were estimated through a "Comprehensive Inversion" of the first 20.5 months of magnetic measurements from European Space Agency's (ESA) Swarm satellite constellation mission. While the constellation provides important north-south along-track gradiometry information, it is the unique low-spacecraft pair that allows for east-west cross-track gradiometry. This latter type is crucial in delivering an M-2 estimate of similar quality with that derived from over 10 years of CHAMP satellite data but over a shorter interval, at higher altitude, and during more magnetically disturbed conditions. Recovered N-2 contains nonoceanic signal but is highly correlated with theoretical models in regions of maximum oceanic amplitude. Thus, satellite magnetic gradiometry may eventually enable the monitoring of ocean electrodynamic properties at temporal resolutions of 1 to 2 years, which may have important implications for the inference of ocean temperature and salinity.
C1 [Sabaka, Terence J.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Tyler, Robert H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Olsen, Nils] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
RP Sabaka, TJ (reprint author), NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM Terence.J.Sabaka@nasa.gov
RI Olsen, Nils/H-1822-2011
OI Olsen, Nils/0000-0003-1132-6113
FU NASA Earth Surface and Interior program; ESA's STSE program
FX We would like to thank ESA for access to the Swarm Level 1b data. We
would also like to thank the staff of the geomagnetic observatories and
INTERMAGNET for supplying high-quality observatory data. We thank two
anonymous reviewers for their valuable comments, and we thank Richard
Ray for useful discussions and for providing Greenwich phase calculation
software. Several figures were generated using the Generic Mapping Tools
(GMT) package [Wessel and Smith, 1991]. The NASA Center for Climate
Simulation at Goddard Space Flight Center provided computational
resources. T.J.S. and R.H.T. are supported by the NASA Earth Surface and
Interior program, and N.O. is supported by ESA's STSE program. Swarm
Level 1b data are available from ESA at http://earth.esa.int/swarm, and
the tidal coefficients of CI1 are available by contacting the authors
directly.
NR 30
TC 2
Z9 2
U1 9
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2016
VL 43
IS 7
BP 3237
EP 3245
DI 10.1002/2016GL068180
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DL3MG
UT WOS:000375537300028
ER
PT J
AU Chew, C
Shah, R
Zuffada, C
Hajj, G
Masters, D
Mannucci, AJ
AF Chew, Clara
Shah, Rashmi
Zuffada, Cinzia
Hajj, George
Masters, Dallas
Mannucci, Anthony J.
TI Demonstrating soil moisture remote sensing with observations from the UK
TechDemoSat-1 satellite mission
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID REFLECTED GPS SIGNALS; SEA-SURFACE; OCEAN; SCATTERING; REFLECTOMETRY;
VEGETATION; MODEL
AB The ability of spaceborne Global Navigation Satellite System(GNSS) bistatic radar receivers to sense changes in soil moisture is investigated using observations from the low Earth orbiting UK TechDemoSat-1 satellite (TDS-1). Previous studies using receivers on aircraft or towers have shown that ground-reflected GNSS signals are sensitive to changes in soil moisture, though the ability to sense this variable from space has yet to be quantified. Data from TDS-1 show a 7 dB sensitivity of reflected signals to temporal changes in soil moisture. If the effects of surface roughness and vegetation on the reflected signals can be quantified, spaceborne GNSS bistatic radar receivers could provide soil moisture on relatively small spatial and temporal scales.
C1 [Chew, Clara; Shah, Rashmi; Zuffada, Cinzia; Hajj, George; Mannucci, Anthony J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Masters, Dallas] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA.
RP Chew, C (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM clara.c.chew@jpl.nasa.gov
FU NASA Postdoctoral Program
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. The authors would like to thank
the members of the TDS-1 team for their hard work in providing the DDMs
used in this study as well as the anonymous reviewers. We would also
like to acknowledge funding from the NASA Postdoctoral Program.
Government sponsorship is acknowledged. Data used in this study were
downloaded from the following sources: GNSS-R data from TDS-1:
www.merrbys.org. SMOS soil moisture and dielectric constant products
were obtained from the "Centre Aval de Traitement des Donnees SMOS"
(CATDS), operated for the "Centre National d'Etudes Spatiales" (CNES,
France) by IFREMER (Brest, France):
http://www.catds.fr/sipad/startPage.do. GLAS canopy height data:
http://webmap.ornl.gov/wcsdown/dataset.jsp?ds_id=10023. MODIS imagery:
https://earthdata.nasa.gov/labs/worldview/. SRTM surface elevation data:
http://srtm.csi.cgiar.org/SELECTION/inputCoord.asp. GlobCover land class
data: http://due.esrin.esa.int/page_globcover.php
NR 29
TC 6
Z9 7
U1 3
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2016
VL 43
IS 7
BP 3317
EP 3324
DI 10.1002/2016GL068189
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DL3MG
UT WOS:000375537300037
ER
PT J
AU Janardanan, R
Maksyutov, S
Oda, T
Saito, M
Kaiser, JW
Ganshin, A
Stohl, A
Matsunaga, T
Yoshida, Y
Yokota, T
AF Janardanan, Rajesh
Maksyutov, Shamil
Oda, Tomohiro
Saito, Makoto
Kaiser, Johannes W.
Ganshin, Alexander
Stohl, Andreas
Matsunaga, Tsuneo
Yoshida, Yukio
Yokota, Tatsuya
TI Comparing GOSAT observations of localized CO2 enhancements by large
emitters with inventory-based estimates
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID PARTICLE DISPERSION MODEL; FOSSIL-FUEL COMBUSTION;
SATELLITE-OBSERVATIONS; EMISSIONS; CHINA; DIOXIDE; VALIDATION; FLEXPART;
BIOMASS; BOTTOM
AB We employed an atmospheric transport model to attribute column-averaged CO2 mixing ratios (X-CO2) observed by Greenhouse gases Observing SATellite (GOSAT) to emissions due to large sources such as megacities and power plants. X-CO2 enhancements estimated from observations were compared to model simulations implemented at the spatial resolution of the satellite observation footprint (0.1 degrees x 0.1 degrees). We found that the simulated X-CO2 enhancements agree with the observed over several continental regions across the globe, for example, for North America with an observation to simulation ratio of 1.05 +/- 0.38 (p < 0.1), but with a larger ratio over East Asia (1.22 +/- 0.32; p < 0.05). The obtained observation-model discrepancy (22%) for East Asia is comparable to the uncertainties in Chinese emission inventories (similar to 15%) suggested by recent reports. Our results suggest that by increasing the number of observations around emission sources, satellite instruments like GOSAT can provide a tool for detecting biases in reported emission inventories.
C1 [Janardanan, Rajesh; Maksyutov, Shamil; Saito, Makoto; Yoshida, Yukio; Yokota, Tatsuya] Natl Inst Environm Studies, Ctr Global Environm Res, Tsukuba, Ibaraki, Japan.
[Oda, Tomohiro] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Oda, Tomohiro] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Kaiser, Johannes W.] Max Planck Inst Chem, Mainz, Germany.
[Ganshin, Alexander] Cent Aerol Observ, Dolgoprudnyi, Russia.
[Ganshin, Alexander] Tomsk State Univ, Tomsk 634050, Russia.
[Stohl, Andreas] NILU Norwegian Inst Air Res, Kjeller, Norway.
[Matsunaga, Tsuneo] Natl Inst Environm Studies, Ctr Environm Measurement & Anal, Tsukuba, Ibaraki, Japan.
RP Janardanan, R (reprint author), Natl Inst Environm Studies, Ctr Global Environm Res, Tsukuba, Ibaraki, Japan.
EM rajesh.janardanan@nies.go.jp
RI Kaiser, Johannes/A-7057-2012; Stohl, Andreas/A-7535-2008;
OI Kaiser, Johannes/0000-0003-3696-9123; Stohl,
Andreas/0000-0002-2524-5755; Maksyutov, Shamil/0000-0002-1200-9577;
Ganshin, Alexander/0000-0002-2835-3145
FU GOSAT project at the National Institute for Environmental Studies,
Japan; Environment Research and Technology Development Fund, Ministry of
Environment Japan [2-1401]
FX The authors are grateful to the GOSAT project at the National Institute
for Environmental Studies, Japan, for support and providing the GOSAT
Level 2 XCO2 data. The supercomputer facility and GOSAT
Research Computation Facility at the National Institute for
Environmental Studies are acknowledged for enabling the simulations.
Study was supported by grant 2-1401 of Environment Research and
Technology Development Fund, Ministry of Environment Japan. The two
anonymous reviewers are gratefully acknowledged.
NR 30
TC 2
Z9 2
U1 4
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2016
VL 43
IS 7
BP 3486
EP 3493
DI 10.1002/2016GL067843
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DL3MG
UT WOS:000375537300057
ER
PT J
AU Liu, JJ
Bowman, K
AF Liu, Junjie
Bowman, Kevin
TI A method for independent validation of surface fluxes from atmospheric
inversion: Application to CO2
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID COLUMN OBSERVING NETWORK; OBSERVATION IMPACT; TRANSPORT; ADJOINT; MODELS
AB Validating fluxes from an atmospheric inversion is a challenging problem because there are often no direct flux measurements at comparable spatiotemporal scales whereas there are often relevant independent observables, e.g., trace gas concentrations. In this paper, we propose a method that validates posterior fluxes by projecting the errors between posterior and prior observable model states and independent data to the spatiotemporal differences between posterior and prior fluxes with an atmospheric transport adjoint model. We prove theoretically the conditions for which observed error reductions lead to error reductions in fluxes. We apply this approach to the atmospheric CO2 inversion problem using the NASA Carbon Monitoring System Flux project with an Observing System Simulation Experiment. We show that the posterior fluxes are more accurate than the prior over the region that significantly contributes to the reduction of CO2 errors, which is consistent with the theory.
C1 [Liu, Junjie; Bowman, Kevin] CALTECH, Jet Prop Lab, La Canada Flintridge, CA USA.
RP Liu, JJ (reprint author), CALTECH, Jet Prop Lab, La Canada Flintridge, CA USA.
EM junjie.liu@jpl.nasa.gov
FU OCO-2 science team grant [NNH11ZDA001N-OCO2]; NASA Carbon Monitoring
System grant [NNH14ZDA001N-CMS]
FX Data to support this article can be obtained by contacting the
corresponding author by email (junjie.liu@jpl.nasa.gov). We acknowledge
the funding support from OCO-2 science team grant (NNH11ZDA001N-OCO2)
and NASA Carbon Monitoring System grant (NNH14ZDA001N-CMS). This
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. All the computations were performed in NASA
AMES supercomputers.
NR 17
TC 0
Z9 0
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2016
VL 43
IS 7
BP 3502
EP 3508
DI 10.1002/2016GL067828
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DL3MG
UT WOS:000375537300059
ER
PT J
AU Schnell, JL
Prather, MJ
Josse, B
Naik, V
Horowitz, LW
Zeng, G
Shindell, DT
Faluvegi, G
AF Schnell, Jordan L.
Prather, Michael J.
Josse, Beatrice
Naik, Vaishali
Horowitz, Larry W.
Zeng, Guang
Shindell, Drew T.
Faluvegi, Greg
TI Effect of climate change on surface ozone over North America, Europe,
and East Asia
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID INTERCOMPARISON PROJECT ACCMIP; REGIONAL AIR-POLLUTION; UNITED-STATES;
ATMOSPHERIC CHEMISTRY; TROPOSPHERIC OZONE; FUTURE CLIMATE; EMISSIONS
CHANGES; SUMMERTIME OZONE; MODEL; QUALITY
AB The effect of future climate change on surface ozone over North America, Europe, and East Asia is evaluated using present-day (2000s) and future (2100s) hourly surface ozone simulated by four global models. Future climate follows RCP8.5, while methane and anthropogenic ozone precursors are fixed at year 2000 levels. Climate change shifts the seasonal surface ozone peak to earlier in the year and increases the amplitude of the annual cycle. Increases in mean summertime and high-percentile ozone are generally found in polluted environments, while decreases are found in clean environments. We propose that climate change augments the efficiency of precursor emissions to generate surface ozone in polluted regions, thus reducing precursor export to neighboring downwind locations. Even with constant biogenic emissions, climate change causes the largest ozone increases at high percentiles. In most cases, air quality extreme episodes become larger and contain higher ozone levels relative to the rest of the distribution.
C1 [Schnell, Jordan L.; Prather, Michael J.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Josse, Beatrice] CNRS, Ctr Natl Rech Meteorol, Meteo France, GAME CNRM, Toulouse, France.
[Naik, Vaishali] NOAA, UCAR, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Horowitz, Larry W.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Zeng, Guang] Natl Inst Water & Atmospher Res, Lauder, New Zealand.
[Shindell, Drew T.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
[Faluvegi, Greg] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY USA.
[Faluvegi, Greg] Columbia Univ, Columbia Earth Inst, New York, NY USA.
RP Schnell, JL (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
EM jschnell@uci.edu
RI Naik, Vaishali/A-4938-2013
OI Naik, Vaishali/0000-0002-2254-1700
FU NASA [NNX09AJ47G, NNX13AL12G, NNX15AE35G]; DOE [DE-SC0007021]; National
Science Foundation's Graduate Research Fellowship Program [DGE-1321846];
NeSI's collaborator institutions; Ministry of Business, Innovation and
Employment's Research Infrastructure Programme
FX Research at UCI was supported by NASA grants NNX09AJ47G, NNX13AL12G, and
NNX15AE35G and DOE award DE-SC0007021. J.L. Schnell was supported by the
National Science Foundation's Graduate Research Fellowship Program
(DGE-1321846). G. Zeng acknowledges the use of New Zealand's national
HPC facilities that are provided by the NZ eScience Infrastructure and
funded jointly by NeSI's collaborator institutions and through the
Ministry of Business, Innovation and Employment's Research
Infrastructure Programme. We are grateful to the British Atmospheric
Data Centre (BADC), which is part of the NERC National Centre for
Atmospheric Science (NCAS), for collecting and archiving the ACCMIP
data. The hourly ACCMIP data at the models' native resolutions can be
obtained at http://badc.nerc.ac.uk, while the remapped MDA8 ozone data
can be obtained by contacting the corresponding author.
NR 44
TC 4
Z9 4
U1 11
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2016
VL 43
IS 7
BP 3509
EP 3518
DI 10.1002/2016GL068060
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA DL3MG
UT WOS:000375537300060
ER
PT J
AU Damiani, A
Funke, B
Lopez-Puertas, M
Santee, ML
Cordero, RR
Watanabe, S
AF Damiani, Alessandro
Funke, Bernd
Lopez-Puertas, Manuel
Santee, Michelle L.
Cordero, Raul R.
Watanabe, Shingo
TI Energetic particle precipitation: A major driver of the ozone budget in
the Antarctic upper stratosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SOLAR PROTON EVENT; LONG-TERM TRENDS; MIDDLE ATMOSPHERE;
GEOMAGNETIC-ACTIVITY; POLAR VORTEX; VARIABILITY; TRANSPORT; CYCLE;
ALGORITHM; NOX
AB Geomagnetic activity is thought to affect ozone and, possibly, climate in polar regions via energetic particle precipitation (EPP) but observational evidence of its importance in the seasonal stratospheric ozone variation on long time scales is still lacking. Here we fill this gap by showing that at high southern latitudes, late winter ozone series, covering the 1979-2014 period, exhibit an average stratospheric depletion of about 10-15% on a monthly basis caused by EPP. Daily observations indicate that every austral winter EPP-induced low ozone concentrations appear at about 45 km in late June and descend later to 30 km, before disappearing by September. Such stratospheric variations are coupled with mesospheric ozone changes also driven by EPP. No significant correlation between these ozone variations and solar ultraviolet irradiance has been found. This suggests the need of including the EPP forcing in both ozone model simulations and trend analysis.
C1 [Damiani, Alessandro; Watanabe, Shingo] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa, Japan.
[Funke, Bernd; Lopez-Puertas, Manuel] CSIC, Inst Astrofis Andalucia, Granada, Spain.
[Santee, Michelle L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Cordero, Raul R.] Univ Santiago Chile, Dept Phys, Santiago, Chile.
RP Damiani, A (reprint author), Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa, Japan.
EM alecarlo.damiani@gmail.com
RI Funke, Bernd/C-2162-2008; Watanabe, Shingo/L-9689-2014
OI Funke, Bernd/0000-0003-0462-4702; Watanabe, Shingo/0000-0002-2228-0088
FU SOUSEI program, MEXT, JAPAN; Spanish MINECO [ESP2014-54362-P]; EC FEDER
funds; FONDECYT [1140239]
FX The present study was supported by the SOUSEI program, MEXT, JAPAN. The
IAA team was supported by the Spanish MINECO under grant ESP2014-54362-P
and EC FEDER funds. Work at the Jet Propulsion Laboratory, California
Institute of Technology, was done under contract with NASA. The Chilean
team was supported by FONDECYT (1140239). MLS/Aura data are available at
the Jet Propulsion Laboratory MLS website:
http://mls.jpl.nasa.gov/index.php. SBUV MOD data are available at
http://acd-ext.gsfc.nasa.gov/Data_services/merged/, and SBUV merged
cohesive data are available at ftp://ftp.cpc.ncep.noaa.gov/SBUV_CDR/.
Zonal means computations within the equivalent latitudes or polar vortex
edge are based on the derived meteorological products for MLS v3.3 data
calculated from GEOS5-based Modern Era-Retrospective Analysis for
Research and Applications (MERRA) reanalysis.
NR 40
TC 2
Z9 2
U1 1
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2016
VL 43
IS 7
BP 3554
EP 3562
DI 10.1002/2016GL068279
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DL3MG
UT WOS:000375537300065
ER
PT J
AU Fortenberry, RC
Roueff, E
Lee, TJ
AF Fortenberry, Ryan C.
Roueff, Evelyne
Lee, Timothy J.
TI Inclusion of C-13 and D in protonated acetylene
SO CHEMICAL PHYSICS LETTERS
LA English
DT Article
ID QUARTIC FORCE-FIELDS; VIBRATIONAL FREQUENCIES; SPECTROSCOPIC CONSTANTS;
INFRARED-SPECTROSCOPY; C2H3+; MOLECULES; ENERGIES; ISOTOPOLOGUES;
INTENSITIES; EXTENSIONS
AB The rovibrational spectrum of cyclic, protonated acetylene has been established. The improvement in modern telescopes coupled with the different branching ratios in reaction models welcomes study of C-13-substitution for C2H3+. Quartic force fields (QFFs) have been previously utilized to predict the anti-symmetric HCCH stretch in standard c-C2H3+ to within 0.1 cm(-1) of experiment and are employed here to generate rovibrational insights for the C-13 isotopologues. The zero-point energies are also given for the cyclic and 'Y'-shaped isomers for both C-13 and D substitutions. Vibrational intensities and the dipole moments are provided in order to characterize more fully this simple cation. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Fortenberry, Ryan C.] Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA.
[Roueff, Evelyne] Univ Paris 06, Sorbonne Univ, Observ Paris, LERMA,PSL Res Univ,CNRS, F-92190 Meudon, France.
[Lee, Timothy J.] NASA, Ames Res Ctr, Mail Stop 245-1, Moffett Field, CA 94035 USA.
RP Fortenberry, RC (reprint author), Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA.
EM rfortenberry@georgiasouthern.edu
RI Lee, Timothy/K-2838-2012
FU Georgia Southern University; Programme National de Physique et Chimie
Interstellaire (PCMI); Agence Nationale de la recherche (ANR) [IMOLABS
ANR-13-BS05-0008]; National Aeronautics and Space Administration through
the NASA Astrobiology Institute [NNH13ZDA017C]
FX Georgia Southern University is acknowledged for start-up funds necessary
for this research. ER acknowledges support from the Programme National
de Physique et Chimie Interstellaire (PCMI) and the Agence Nationale de
la recherche (ANR) through the ResearAgencech project IMOLABS
ANR-13-BS05-0008. This work is also supported by the National
Aeronautics and Space Administration through the NASA Astrobiology
Institute under Cooperative Agreement Notice NNH13ZDA017C issued through
the Science Mission Directorate.
NR 42
TC 3
Z9 3
U1 1
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2614
EI 1873-4448
J9 CHEM PHYS LETT
JI Chem. Phys. Lett.
PD APR 16
PY 2016
VL 650
BP 126
EP 129
DI 10.1016/j.cplett.2016.02.068
PG 4
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DK5NP
UT WOS:000374966900025
ER
PT J
AU McGrath-Spangler, EL
AF McGrath-Spangler, E. L.
TI The impact of a boundary layer height formulation on the GEOS-5 model
climate (Retracted article. See vol. 121, pg. 5749, 2016)
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE planetary boundary layer; turbulence; global modeling; climate
ID BOREAL FOREST; CIRCULATION; CONVECTION; TRANSPORT; DYNAMICS; AGCM
AB Planetary boundary layer (PBL) processes are important for the estimation of surface-atmosphere exchanges that impact global climate. One way of characterizing the strength of these processes is the PBL depth. In the Goddard Earth Observing System (GEOS-5) atmospheric general circulation model, the PBL depth is also used in calculating the turbulent length scale, which, in turn, is used in estimating the turbulence and vertical mixing within the model. Therefore, changing the PBL depth definition directly affects the model climate. This study evaluates the climatological model response of two long-term simulations using different PBL depth definitions. The first definition is based on a bulk Richardson number; the second uses a combination of the same bulk Richardson number definition over land plus a definition based on the turbulent eddy diffusion coefficient over water. The two simulations produce different spatiotemporal patterns of temperature, specific humidity, and wind speed related to the differences in turbulence. The largest differences, as expected, are present over water. Due to differences in atmospheric stability, the relationship between the two PBL depth estimates differ among the majority of the oceans and off the west coasts of continents, affecting the climatic response. Due to its optimization of the climatic response while maintaining a realistic diurnal cycle of PBL depth, the mixed PBL depth configuration is preferred.
C1 [McGrath-Spangler, E. L.] Univ Space Res Assoc, Columbia, MD USA.
[McGrath-Spangler, E. L.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
RP McGrath-Spangler, EL (reprint author), Univ Space Res Assoc, Columbia, MD USA.; McGrath-Spangler, EL (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
EM erica.l.mcgrath-spangler@nasa.gov
OI McGrath-Spangler, Erica/0000-0002-8540-5423
FU National Aeronautics and Space Administration [NNX15AE62G]
FX The author thanks two anonymous reviewers whose suggestions helped to
improve this manuscript. The GEOS-5 source code is available from the
NASA Global Modeling and Assimilation Office. The MERRA-2 data are
produced by the NASA Global Modeling and Assimilation Office and
disseminated by the GES DISC with support from NASA's Modeling,
Analysis, and Prediction program. Computing was supported by allocations
on the NASA Center for Climate Simulation from Tsengdar Lee. The
research was supported by Richard Eckman through National Aeronautics
and Space Administration grant NNX15AE62G.
NR 29
TC 1
Z9 1
U1 5
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2016
VL 121
IS 7
BP 3263
EP 3275
DI 10.1002/2015JD024607
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DK7QG
UT WOS:000375120200011
ER
PT J
AU Ge, C
Wang, J
Carn, S
Yang, K
Ginoux, P
Krotkov, N
AF Ge, Cui
Wang, Jun
Carn, Simon
Yang, Kai
Ginoux, Paul
Krotkov, Nickolay
TI Satellite-based global volcanic SO2 emissions and sulfate direct
radiative forcing during 2005-2012
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE OMI SO2; volcanic sulfate aerosols; direct radiative forcing; injection
height; volcanic emission inventory; volcanic degassing
ID OZONE MONITORING INSTRUMENT; SULFUR-DIOXIDE EMISSIONS; SIERRA-NEGRA
VOLCANO; 2005 ERUPTION; EAST-ASIA; AEROSOL; CLIMATE; OMI; CLOUDS; MODEL
AB An 8year volcanic SO2 emission inventory for 2005-2012 is obtained based on satellite measurements of SO2 from OMI (Ozone Monitoring Instrument) and ancillary information from the Global Volcanism Program. It includes contributions from global volcanic eruptions and from eight persistently degassing volcanoes in the tropics. It shows significant differences in the estimate of SO2 amount and injection height for medium to large volcanic eruptions as compared to the counterparts in the existing volcanic SO2 database. Emissions from Nyamuragira (DR Congo) in November 2006 and Grimsvotn (Iceland) in May 2011 that were not included in the Intergovernmental Panel on Climate Change 5 (IPCC) inventory are included here. Using the updated emissions, the volcanic sulfate (SO42-) distribution is simulated with the global transport model Goddard Earth Observing System (GEOS)-Chem. The simulated time series of sulfate aerosol optical depth (AOD) above 10km captures every eruptive volcanic sulfate perturbation with a similar magnitude to that measured by Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO). The 8year average contribution of eruptive SO42- to total SO42- loading above 10km is similar to 10% over most areas of the Northern Hemisphere, with a maxima of 30% in the tropics where the anthropogenic emissions are relatively smaller. The persistently degassing volcanic SO42- in the tropics barely reaches above 10km, but in the lower atmosphere it is regionally dominant (60%+ in terms of mass) over Hawaii and other oceanic areas northeast of Australia. Although the 7year average (2005-2011) of eruptive volcanic sulfate forcing of -0.10Wm(-2) in this study is comparable to that in the 2013 IPCC report (-0.09Wm(-2)), significant discrepancies exist for each year. Our simulations also imply that the radiative forcing per unit AOD for volcanic eruptions can vary from -40 to -80Wm(-2), much higher than the -25Wm(-2) implied in the IPCC calculations. In terms of sulfate forcing efficiency with respect to SO2 emission, eruptive volcanic sulfate is 5 times larger than anthropogenic sulfate. The sulfate forcing efficiency from degassing volcanic sources is close to that of anthropogenic sources. This study highlights the importance of characterizing both volcanic emission amount and injection altitude as well as the key role of satellite observations in maintaining accurate volcanic emissions inventories.
C1 [Ge, Cui; Wang, Jun] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA.
[Carn, Simon] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA.
[Yang, Kai] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Ginoux, Paul] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Krotkov, Nickolay] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA.
RP Wang, J (reprint author), Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA.
EM jwang7@unl.edu
RI Ge, Cui/I-6353-2016; Krotkov, Nickolay/E-1541-2012; Chem,
GEOS/C-5595-2014; Ginoux, Paul/C-2326-2008; Wang, Jun/A-2977-2008
OI Ge, Cui/0000-0002-6182-6856; Krotkov, Nickolay/0000-0001-6170-6750;
Ginoux, Paul/0000-0003-3642-2988; Wang, Jun/0000-0002-7334-0490
FU NASA [NNX10AG60G]
FX Levi Boggs and Frances Wiles are acknowledged for their work on
collecting the volcano injection altitudes data. The authors gratefully
acknowledge the Smithsonian Global Volcanism Program, Thomas Diehl, Tom
Simkin, and Lee Siebert for providing AeroCom volcano emission data. We
appreciate Brendam McCormick and two other reviewers for their
constructive comments. The authors thank the Holland Computing Center of
University of Nebraska-Lincoln, its director David Swanson, and his
staff Adam Caprez and Jingchao Zhang for their helpful efforts with
modeling work. The GEOS-Chem developers and support team in Harvard
University are acknowledged for their help. This work is supported by
NASA Atmospheric Chemistry Modeling and Analysis Program (NNX10AG60G)
managed by Richard S. Eckman, NASA Atmospheric Composition program, and
Radiation Sciences Program managed by Hal B. Maring. Data shown in the
paper can be obtained from the corresponding author through e-mail
(jwang7@unl.edu), and part of the emission data can be obtained from
ftp://measures.gsfc.nasa.gov/data/s4pa/SO2/MSVOLSO2L4.1/MSVOLSO2L4_v01-0
0-2014m1002.txt.
NR 102
TC 2
Z9 2
U1 8
U2 19
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2016
VL 121
IS 7
BP 3446
EP 3464
DI 10.1002/2015JD023134
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DK7QG
UT WOS:000375120200023
ER
PT J
AU Ott, LE
Duncan, BN
Thompson, AM
Diskin, G
Fasnacht, Z
Langford, AO
Lin, MY
Molod, AM
Nielsen, JE
Pusede, SE
Wargan, K
Weinheimer, AJ
Yoshida, Y
AF Ott, Lesley E.
Duncan, Bryan N.
Thompson, Anne M.
Diskin, Glenn
Fasnacht, Zachary
Langford, Andrew O.
Lin, Meiyun
Molod, Andrea M.
Nielsen, J. Eric
Pusede, Sally E.
Wargan, Krzysztof
Weinheimer, Andrew J.
Yoshida, Yasuko
TI Frequency and impact of summertime stratospheric intrusions over
Maryland during DISCOVER-AQ (2011): New evidence from NASA's GEOS-5
simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE ozone; stratospheric intrusion; air quality
ID LONG-RANGE TRANSPORT; TROPOSPHERE EXCHANGE; OZONE CONCENTRATIONS; GLOBAL
CLIMATOLOGY; BACKGROUND OZONE; TROPOPAUSE FOLDS; UNITED-STATES;
PACIFIC-OCEAN; AIR-QUALITY; SURFACE AIR
AB Aircraft observations and ozonesonde profiles collected on 14 and 27 July 2011, during the Maryland month-long Deriving Information on Surface conditions from Column and Vertically Resolved Observations Relevant to Air Quality (DISCOVER-AQ) campaign, indicate the presence of stratospheric air just above the planetary boundary layer (PBL). This raises the question of whether summer stratospheric intrusions (SIs) elevate surface ozone levels and to what degree they influence background ozone levels and contribute to ozone production. We used idealized stratospheric air tracers, along with observations, to determine the frequency and extent of SIs in Maryland during July 2011. On 4 of 14 flight days, SIs were detected in layers that the aircraft encountered above the PBL from the coincidence of enhanced ozone, moderate CO, and low moisture. Satellite observations of lower tropospheric humidity confirmed the occurrence of synoptic-scale influence of SIs as do simulations with the GEOS-5 atmospheric general circulation model. The evolution of GEOS-5 stratospheric air tracers agrees with the timing and location of observed stratospheric influence and indicates that more than 50% of air in SI layers above the PBL had resided in the stratosphere within the previous 14days. Despite having a strong influence in the lower free troposphere, these events did not significantly affect surface ozone, which remained low on intrusion days. The model indicates similar frequencies of stratospheric influence during all summers from 2009 to 2013. GEOS-5 results suggest that over Maryland, the strong inversion capping the summer PBL limits downward mixing of stratospheric air during much of the day, helping to preserve low surface ozone associated with frontal passages that precede SIs.
C1 [Ott, Lesley E.; Duncan, Bryan N.; Thompson, Anne M.; Molod, Andrea M.; Nielsen, J. Eric; Wargan, Krzysztof; Yoshida, Yasuko] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Diskin, Glenn] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Fasnacht, Zachary] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Langford, Andrew O.] NOAA, Earth Syst Res Lab, Chem Sci Div, Boulder, CO USA.
[Lin, Meiyun] Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA.
[Lin, Meiyun] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Molod, Andrea M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Nielsen, J. Eric; Wargan, Krzysztof; Yoshida, Yasuko] Sci Syst & Applicat Inc, Lanham, MD USA.
[Pusede, Sally E.] Univ Virginia, Dept Environm Sci, Clark Hall, Charlottesville, VA 22903 USA.
[Weinheimer, Andrew J.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
RP Ott, LE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM lesley.e.ott@nasa.gov
RI Lin, Meiyun/D-6107-2013; Langford, Andrew/D-2323-2009; Ott,
Lesley/E-2250-2012; Duncan, Bryan/A-5962-2011; Manager, CSD
Publications/B-2789-2015; Thompson, Anne /C-3649-2014;
OI Lin, Meiyun/0000-0003-3852-3491; Langford, Andrew/0000-0002-2932-7061;
Thompson, Anne /0000-0002-7829-0920; Wargan,
Krzysztof/0000-0002-3795-2983
FU NASA's Atmospheric Composition Campaign Data Analysis and Modeling
program; NASA's DISCOVER-AQ campaign
FX This work was supported by funding from NASA's Atmospheric Composition
Campaign Data Analysis and Modeling program and NASA's DISCOVER-AQ
campaign. MERRA and MERRA-2 data have been provided by the GMAO at
NASA's Goddard Space Flight Center through the NASA GES DISC online
archive. AIRS data are also available through the GES DISC. DISCOVER-AQ
aircraft and ozonesonde observations were provided by NASA's Langley
Research Center at
http://www-air.larc.nasa.gov/missions/discover-aq/discover-aq.html.
GEOS-5 stratospheric tracer simulations will be provided upon request.
NR 78
TC 4
Z9 4
U1 5
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2016
VL 121
IS 7
BP 3687
EP 3706
DI 10.1002/2015JD024052
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DK7QG
UT WOS:000375120200038
ER
PT J
AU Plane, JMC
Gomez-Martin, JC
Feng, WH
Janches, D
AF Plane, John M. C.
Gomez-Martin, Juan Carlos
Feng, Wuhu
Janches, Diego
TI Silicon chemistry in the mesosphere and lower thermosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE silicon chemistry; meteoric ablation; mesospheric ions
ID POSITIVE-ION COMPOSITION; COSMIC DUST; EARTHS ATMOSPHERE; D-REGION;
MODEL; IONOSPHERE; SI+; RECOMBINATION; PARTICLES; VELOCITY
AB Silicon is one of the most abundant elements in cosmic dust, and meteoric ablation injects a significant amount of Si into the atmosphere above 80km. In this study, a new model for silicon chemistry in the mesosphere/lower thermosphere is described, based on recent laboratory kinetic studies of Si, SiO, SiO2, and Si+. Electronic structure calculations and statistical rate theory are used to show that the likely fate of SiO2 is a two-step hydration to silicic acid (Si(OH)(4)), which then polymerizes with metal oxides and hydroxides to form meteoric smoke particles. This chemistry is then incorporated into a whole atmosphere chemistry-climate model. The vertical profiles of Si+ and the Si+/Fe+ ratio are shown to be in good agreement with rocket-borne mass spectrometric measurements between 90 and 110km. Si+ has consistently been observed to be the major meteoric ion around 110km; this implies that the relative injection rate of Si from meteoric ablation, compared to metals such as Fe and Mg, is significantly larger than expected based on their relative chondritic abundances. Finally, the global abundances of SiO and Si(OH)(4) show clear evidence of the seasonal meteoric input function, which is much less pronounced in the case of other meteoric species.
C1 [Plane, John M. C.; Gomez-Martin, Juan Carlos; Feng, Wuhu] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England.
[Feng, Wuhu] Univ Leeds, NCAS, Leeds, W Yorkshire, England.
[Feng, Wuhu] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England.
[Janches, Diego] NASA, GSFC, Space Weather Lab, Greenbelt, MD USA.
RP Plane, JMC (reprint author), Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England.
EM J.M.C.Plane@leeds.ac.uk
RI Plane, John/C-7444-2015; Janches, Diego/D-4674-2012; FENG,
WUHU/B-8327-2008
OI Gomez Martin, Juan Carlos/0000-0001-7972-085X; Plane,
John/0000-0003-3648-6893; Janches, Diego/0000-0001-8615-5166; FENG,
WUHU/0000-0002-9907-9120
FU European Research Council [291332-CODITA]; NASA [12-PAST12-0007,
12-PATM12-0006]
FX This work was supported by the European Research Council (project
291332-CODITA). D.J. is supported by NASA awards 12-PAST12-0007 and
12-PATM12-0006. The mass spectrometric data (kindly provided by E. Kopp)
and WACCM data sets are available upon request to J.M.C.P.
NR 54
TC 2
Z9 2
U1 4
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2016
VL 121
IS 7
BP 3718
EP 3728
DI 10.1002/2015JD024691
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DK7QG
UT WOS:000375120200040
PM 27668138
ER
PT J
AU Schmidt, ME
Schrader, CM
Crumpler, LS
Rowe, MC
Wolff, JA
Boroughs, SP
AF Schmidt, Mariek E.
Schrader, Christian M.
Crumpler, Larry S.
Rowe, Michael C.
Wolff, John A.
Boroughs, Scott P.
TI Megacrystic pyroxene basalts sample deep crustal gabbroic cumulates
beneath the Mount Taylor volcanic field, New Mexico
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Review
DE Pyroxene; Plagioclase; Alkali basalt; Sr-87/Sr-86; New Mexico
ID RIO-GRANDE RIFT; WESTERN UNITED-STATES; COLORADO PLATEAU; TOPAZ
RHYOLITES; CHILEAN ANDES; ZUNI-BANDERA; ARC; EVOLUTION; ZONE; USA
AB Distributed over the similar to 2.3 m.y. history of the alkaline and compositionally diverse Mount Taylor Volcanic Field (MTVF), New Mexico is a widespread texturally distinct family of differentiated basalts that contain resorbed megacrysts (up to 3 cm) of plagioclase, clinopyroxene, and olivine +/- Ti-magnetite +/- ilmenite +/- orthopyroxene. These lavas have gabbroic cumulate inclusions with mineral compositions similar to the megacrysts, suggesting a common origin. Gabbroic and megacrystic clinopyroxenes form positive linear arrays in TiO2 (0.2-23 wt%) with respect to Al2O3 (0.7-9.3 wt.%). Plagioclase (An(41-80)) from representative thin sections analyzed for Sr-87/Sr-86 by laser ablation ICP-MS range from 0.7036 to 0.7048. The low Sr-87/Sr-86 plagioclases (0.7036 to 0.7037) are associated with high Ti-Al clinopyroxenes. Likewise, the higher Sr-87/Sr-86 plagioclases (0.7043 to 0.7047) are associated with the low-Al clinopyroxenes. Taken together, the pyroxene and plagioclase megacrysts appear to track the differentiation of a gabbroic pluton (or related plutons) from alkaline to Si-saturated conditions by fractional crystallization and crustal assimilation. Clinopyroxene-liquid geobarometry calculations suggest that crystallization occurred near the crust-mantle transition at an average of similar to 1200 degrees C and 12-13 kbar. The distribution of the megacrystic pyroxene basalts suggests that a gabbroic intrusive body underlies subregions of the MTVF that have generated silicic magmas. The gabbro is interpreted to be a significant heat and mass input into the lower crust that is capable of driving the petrogenesis of diverse silicic compositions (through fractionation and crustal assimilation), including mugearites, trachytes, trachy-andesites and dacites, high-Si rhyolites, and topaz rhyolites of the MTVF. (C) 2016 The Authors. Published by Elsevier B.V.
C1 [Schmidt, Mariek E.] Brock Univ, Dept Earth Sci, 500 Glenridge Ave, St Catharines, ON L2S 3A1, Canada.
[Schrader, Christian M.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Schrader, Christian M.] Bowdoin Coll, Earth & Oceanog Sci, Brunswick, ME 04011 USA.
[Crumpler, Larry S.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA.
[Rowe, Michael C.] Univ Auckland, Sch Environm, Auckland 1142, New Zealand.
[Wolff, John A.; Boroughs, Scott P.] Washington State Univ, Sch Environm, Pullman, WA 99164 USA.
RP Schmidt, ME (reprint author), Brock Univ, Dept Earth Sci, 500 Glenridge Ave, St Catharines, ON L2S 3A1, Canada.
EM mschmidt2@brocku.ca; cschrade@bowdoin.edu; larry.crumpler@state.nm.us;
michael.rowe@auckland.ac.nz; jawolff@wsu.edu; scott.boroughs@wsu.edu
FU NSERC Discovery Grant [385995]; NASA Postdoctoral Fellowship
FX This work was supported by NSERC Discovery Grant (#385995) to Schmidt
and a NASA Postdoctoral Fellowship to Schrader. Two anonymous reviewers
provided insightful and helpful comments. We thank Drew Coleman and one
anonymous reviewer who provided comments on an earlier draft. We thank
Alicia Thomas and Jayne Aubel for field assistance and Emma Bullock who
aided with analyses. We are also very grateful to Jack Farley who
provided access to Grants Ridge.
NR 42
TC 0
Z9 0
U1 4
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0273
EI 1872-6097
J9 J VOLCANOL GEOTH RES
JI J. Volcanol. Geotherm. Res.
PD APR 15
PY 2016
VL 316
BP 1
EP 11
DI 10.1016/j.jvolgeores.2016.02.020
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA DN1QE
UT WOS:000376839700001
ER
PT J
AU Tompson, SR
AF Tompson, Sara R.
TI The Copyright Librarian: A Practical Handbook
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Tompson, Sara R.] Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA USA.
RP Tompson, SR (reprint author), Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA USA.
NR 1
TC 0
Z9 0
U1 1
U2 1
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD APR 15
PY 2016
VL 141
IS 7
BP 103
EP 103
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA DJ8BM
UT WOS:000374437100190
ER
PT J
AU Stuart, J
Howell, K
Wilson, R
AF Stuart, Jeffrey
Howell, Kathleen
Wilson, Roby
TI Application of multi-agent coordination methods to the design of space
debris mitigation tours
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Automated trajectory design; Space debris mitigation; Ant colony
optimization; Multi-agent auctions; Vehicle routing problem
ID REMOVAL; ALGORITHM
AB The growth in the number of defunct and fragmented objects near to the Earth poses a growing hazard to launch operations as well as existing on-orbit assets. Numerous studies have demonstrated the positive impact of active debris mitigation campaigns upon the growth of debris populations, but comparatively fewer investigations incorporate specific mission scenarios. Furthermore, while many active mitigation methods have been proposed, certain classes of debris objects are amenable to mitigation campaigns employing chaser spacecraft with existing chemical and low-thrust propulsive technologies. This investigation incorporates an ant colony optimization routing algorithm and multi-agent coordination via auctions into a debris mitigation tour scheme suitable for preliminary mission design and analysis as well as spacecraft flight operations. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Stuart, Jeffrey; Howell, Kathleen] Purdue Univ, Sch Aeronaut & Astronaut, 701 W Stadium Ave, W Lafayette, IN 47906 USA.
[Wilson, Roby] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Stuart, J (reprint author), CALTECH, Jet Prop Lab, Miss Design & Nav Sect, Nav & Miss Design Syst Engn Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jeffrey.r.stuart@jpl.nasa.gov; howell@purdue.edu;
roby.s.wilson@jpl.nasa.gov
FU NASA Office of the Chief Technologist's Space Technology Research
Fellowship; NASA [NNX12AM61H]; Purdue Research Foundation
FX This research was conducted at Purdue University and the Jet Propulsion
Laboratory, California Institute of Technology under contract with the
National Aeronautics and Space Administration. The work was supported by
a NASA Office of the Chief Technologist's Space Technology Research
Fellowship, NASA Grant NNX12AM61H, and the Purdue Research Foundation.
Many thanks to Wayne Schlei, for the many discussions on ACO and
auctions, and the technical personnel at the Jet Propulsion Laboratory,
Mission Design and Navigation Section. The authors also acknowledge the
contributions of Professor Seokcheon Lee of the Purdue University School
of Industrial Engineering.
NR 30
TC 1
Z9 1
U1 2
U2 4
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 15
PY 2016
VL 57
IS 8
BP 1680
EP 1697
DI 10.1016/j.asr.2015.05.002
PG 18
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA DJ7CH
UT WOS:000374369000007
ER
PT J
AU Carroll, BE
Otis, RA
Borgonia, JP
Suh, JO
Dillon, RP
Shapiro, AA
Hofmann, DC
Liu, ZK
Beese, AM
AF Carroll, Beth E.
Otis, Richard A.
Borgonia, John Paul
Suh, Jong-ook
Dillon, R. Peter
Shapiro, Andrew A.
Hofmann, Douglas C.
Liu, Zi-Kui
Beese, Allison M.
TI Functionally graded material of 304L stainless steel and inconel 625
fabricated by directed energy deposition: Characterization and
thermodynamic modeling
SO ACTA MATERIALIA
LA English
DT Article
DE Additive manufacturing; Functionally graded material; Thermodynamic
modeling; Laser deposition; Microstructure
ID DIRECT METAL-DEPOSITION; MICROSTRUCTURAL EVOLUTION;
MECHANICAL-PROPERTIES; STRUCTURAL MATERIAL; TITANIUM-VANADIUM; LASER;
ALLOYS; BEAM; COMPOSITES; PARTS
AB Many engineering applications, particularly in extreme environments, require components with properties that vary with location in the part. Functionally graded materials (FGMs), which possess gradients in properties such as hardness or density, are a potential solution to address these requirements. The laser-based additive manufacturing process of directed energy deposition (DED) can be used to fabricate metallic parts with a gradient in composition by adjusting the volume fraction of metallic powders delivered to the melt pool as a function of position. As this is a fusion process, secondary phases may develop in the gradient zone during solidification that can result in undesirable properties in the part. This work describes experimental and thermodynamic studies of a component built from 304L stainless steel incrementally graded to Inconel 625. The microstructure, chemistry, phase composition, and microhardness as a function of position were characterized by microscopy, energy dispersive spectros-copy, X-ray diffraction, and microindentation. Particles of secondary phases were found in small amounts within cracks in the gradient zone. These were ascertained to consist of transition metal carbides by experimental results and thermodynamic calculations. The study provides a combined experimental and thermodynamic computational modeling approach toward the fabrication and evaluation of a functionally graded material made by DED additive manufacturing. (C) 2016 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Carroll, Beth E.; Otis, Richard A.; Liu, Zi-Kui; Beese, Allison M.] Penn State Univ, Dept Mat Sci & Engn, University Pk, PA 16802 USA.
[Borgonia, John Paul; Suh, Jong-ook; Dillon, R. Peter; Shapiro, Andrew A.; Hofmann, Douglas C.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Beese, AM (reprint author), Penn State Univ, Dept Mat Sci & Engn, University Pk, PA 16802 USA.
EM amb961@psu.edu
RI Liu, Zi-Kui/A-8196-2009;
OI Liu, Zi-Kui/0000-0003-3346-3696; Otis, Richard/0000-0002-1147-9032;
Beese, Allison/0000-0002-7022-3387
FU National Science Foundation [CMMI-1402978]; NASA Space Technology
Research Fellowship [NNX14AL43H]
FX The authors gratefully acknowledge the financial support of the National
Science Foundation through award number CMMI-1402978. Any opinions,
findings, and conclusions or recommendations expressed in this material
are those of the authors and do not necessarily reflect the views of the
National Science Foundation. R.A.O. received funding from a NASA Space
Technology Research Fellowship under grant NNX14AL43H. We also
acknowledge technical assistance from Ashley Reichardt with preliminary
thermodynamic calculations. Part of this research was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration (NASA).
NR 53
TC 1
Z9 1
U1 30
U2 71
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6454
EI 1873-2453
J9 ACTA MATER
JI Acta Mater.
PD APR 15
PY 2016
VL 108
BP 46
EP 54
DI 10.1016/j.actamat.2016.02.019
PG 9
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA DJ2YZ
UT WOS:000374072700006
ER
PT J
AU Bowers, ML
Gao, Y
Yang, L
Gaydosh, D
De Graef, M
Noebe, RD
Wang, Y
Mills, MJ
AF Bowers, M. L.
Gao, Y.
Yang, L.
Gaydosh, D. J.
De Graef, M.
Noebe, R. D.
Wang, Y.
Mills, M. J.
TI Austenite grain refinement during load-biased thermal cycling of a
Ni49.9Ti50.1 shape memory alloy (vol 91 pg 318, 2015)
SO ACTA MATERIALIA
LA English
DT Correction
C1 [Bowers, M. L.; Gao, Y.; Yang, L.; Wang, Y.; Mills, M. J.] Ohio State Univ, Dept Mat Sci & Engn, 116 W 19Th Ave, Columbus, OH 43210 USA.
[De Graef, M.] Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA USA.
[Gaydosh, D. J.; Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
[Gaydosh, D. J.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
RP Bowers, ML (reprint author), Ohio State Univ, Dept Mat Sci & Engn, 116 W 19Th Ave, Columbus, OH 43210 USA.
EM bowers.246@osu.edu
NR 1
TC 0
Z9 0
U1 2
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6454
EI 1873-2453
J9 ACTA MATER
JI Acta Mater.
PD APR 15
PY 2016
VL 108
BP 380
EP 380
DI 10.1016/j.actamat.2016.01.044
PG 1
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA DJ2YZ
UT WOS:000374072700035
ER
PT J
AU Ploutz-Snyder, L
AF Ploutz-Snyder, Lori
TI Evaluating countermeasures in spaceflight analogs
SO JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Review
DE spaceflight; Mars exploration; exercise; bed rest
ID LOWER-LIMB SUSPENSION; BED REST; PARABOLIC FLIGHT; SIMULATED
MICROGRAVITY; EXERCISE; GRAVITY; BONE; WEIGHTLESSNESS; LOCOMOTION;
MIDODRINE
AB Countermeasures are defined as solutions to prevent the undesirable physiologic outcomes associated with spaceflight. Spaceflight analogs provide a valuable opportunity for the evaluation of countermeasures because they allow for the evaluation of more subjects, more experimental control, and are considerably less expensive than actual spaceflight. The various human analogs have differing strengths and weaknesses with respect to the development and evaluation of countermeasures. The human analogs are briefly reviewed with a focus on their suitability for countermeasure evaluation. Bed rest is the most commonly used analog for evaluating countermeasures. While countermeasures are typically developed to target one or maybe two particular physiologic issues, it is increasingly important to evaluate all of the organ systems to discern whether they might be unintended consequences on nontargeted tissues. In preparation for Mars exploration it will be necessary to fully integrate countermeasures to protect all organ systems. The synergistic and antagonistic effects of multiple countermeasures needs to be the focus of future work.
C1 [Ploutz-Snyder, Lori] NASA, Lyndon B Johnson Space Ctr, Exercise Physiol & Countermeasures, Univ Space Res Assoc, Houston, TX 77058 USA.
RP Ploutz-Snyder, L (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,B261 SK3, Houston, TX 77058 USA.
EM lori.ploutz-snyder-1@nasa.gov
NR 49
TC 3
Z9 3
U1 1
U2 1
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 8750-7587
EI 1522-1601
J9 J APPL PHYSIOL
JI J. Appl. Physiol.
PD APR 15
PY 2016
VL 120
IS 8
BP 915
EP 921
DI 10.1152/japplphysiol.00860.2015
PG 7
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA DJ3KD
UT WOS:000374102900011
PM 26662054
ER
PT J
AU Westby, CM
Martin, DS
Lee, SMC
Stenger, MB
Platts, SH
AF Westby, Christian M.
Martin, David S.
Lee, Stuart M. C.
Stenger, Michael B.
Platts, Steven H.
TI Left ventricular remodeling during and after 60 days of sedentary
head-down bed rest
SO JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE echocardiography; cardiac atrophy; cardiovascular physiology; space
flight
ID LONG-DURATION SPACEFLIGHT; TIME 3-DIMENSIONAL ECHOCARDIOGRAPHY;
ORTHOSTATIC INTOLERANCE; CARDIAC ATROPHY; PLASMA-VOLUME; SPACE-FLIGHT;
DIASTOLIC SUCTION; FILLING PRESSURE; MASS; BLOOD
AB Short periods of weightlessness are associated with reduced stroke volume and left ventricular (LV) mass that appear rapidly and are thought to be largely dependent on plasma volume. The magnitude of these cardiac adaptations are even greater after prolonged periods of simulated weightlessness, but the time course during and the recovery from bed rest has not been previously described. We collected serial measures of plasma volume (PV, carbon monoxide rebreathing) and LV structure and function [ tissue Doppler imaging, three-dimensional (3-D) and 2-D echocardiography] before, during, and up to 2 wk after 60 days of 60 head down tilt bed rest (HDTBR) in seven healthy subjects (four men, three women). By 60 days of HDTBR, PV was markedly reduced (2.7 +/- 0.3 vs. 2.3 +/- 0.3 liters, P < 0.001). Resting measures of LV volume and mass were similar to 15% (P < 0.001) and similar to 14% lower (P < 0.001), respectively, compared with pre-HDTBR values. After 3 days of reambulation, both PV and LV volumes were not different than pre-HDTBR values. However, LV mass did not recover with normalization of PV and remained 12 +/- 4% lower than pre-bed rest values (P < 0.001). As previously reported, decreased PV and LV volume precede and likely contribute to cardiac atrophy during prolonged LV unloading. Although PV and LV volume recover rapidly after HDTBR, there is no concomitant normalization of LV mass. These results demonstrate that reduced LV mass in response to prolonged simulated weightlessness is not a simple effect of tissue dehydration, but rather true LV muscle atrophy that persists well into recovery.
C1 [Westby, Christian M.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA.
[Martin, David S.; Lee, Stuart M. C.; Stenger, Michael B.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Platts, Steven H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Platts, SH (reprint author), NASA, Lyndon B Johnson Space Ctr, Biomed Res & Environm Sci, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM steven.platts-1@nasa.gov
FU National Aeronautics and Space Administration Human Research Program
[BRC-2003-0000-0543]; National Center for Advancing Translational
Sciences [1UL-1RR-029876-01]
FX This work was funded by National Aeronautics and Space Administration
Human Research Program Grant BRC-2003-0000-0543 and in part by National
Center for Advancing Translational Sciences Grant 1UL-1RR-029876-01.
NR 63
TC 1
Z9 1
U1 4
U2 6
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 8750-7587
EI 1522-1601
J9 J APPL PHYSIOL
JI J. Appl. Physiol.
PD APR 15
PY 2016
VL 120
IS 8
BP 956
EP 964
DI 10.1152/japplphysiol.00676.2015
PG 9
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA DJ3KD
UT WOS:000374102900016
PM 26494448
ER
PT J
AU Altobelli, N
Postberg, F
Fiege, K
Trieloff, M
Kimura, H
Sterken, VJ
Hsu, HW
Hillier, J
Khawaja, N
Moragas-Klostermeyer, G
Blum, J
Burton, M
Srama, R
Kempf, S
Gruen, E
AF Altobelli, N.
Postberg, F.
Fiege, K.
Trieloff, M.
Kimura, H.
Sterken, V. J.
Hsu, H. -W.
Hillier, J.
Khawaja, N.
Moragas-Klostermeyer, G.
Blum, J.
Burton, M.
Srama, R.
Kempf, S.
Gruen, E.
TI Flux and composition of interstellar dust at Saturn from Cassini's
Cosmic Dust Analyzer
SO SCIENCE
LA English
DT Article
ID IN-SITU MEASUREMENTS; SOLAR-SYSTEM; PRESOLAR GRAINS; HELIOSPHERE;
STARDUST; MICROPARTICLES; NEIGHBORHOOD; SPACECRAFT; ORIGINS; CLOUD
AB Interstellar dust (ISD) is the condensed phase of the interstellar medium. In situ data from the Cosmic Dust Analyzer on board the Cassini spacecraft reveal that the Saturnian system is passed by ISD grains from our immediate interstellar neighborhood, the local interstellar cloud. We determine the mass distribution of 36 interstellar grains, their elemental composition, and a lower limit for the ISD flux at Saturn. Mass spectra and grain dynamics suggest the presence of magnesium-rich grains of silicate and oxide composition, partly with iron inclusions. Major rock-forming elements (magnesium, silicon, iron, and calcium) are present in cosmic abundances, with only small grain-to-grain variations, but sulfur and carbon are depleted. The ISD grains in the solar neighborhood appear to be homogenized, likely by repeated processing in the interstellar medium.
C1 [Altobelli, N.] European Space Agcy, European Space Astron Ctr, Madrid, Spain.
[Postberg, F.; Fiege, K.; Trieloff, M.; Gruen, E.] Heidelberg Univ, Inst Geowissensch, Heidelberg, Germany.
[Postberg, F.; Khawaja, N.; Moragas-Klostermeyer, G.; Srama, R.; Gruen, E.] Univ Stuttgart, Inst Raumfahrtsyst, D-70174 Stuttgart, Germany.
[Fiege, K.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA.
[Trieloff, M.] Heidelberg Univ, Klaus Tschira Labor Kosmochem, Heidelberg, Germany.
[Kimura, H.] Kobe Univ, Kobe, Hyogo 657, Japan.
[Sterken, V. J.] Int Space Sci Inst, Bern, Switzerland.
[Hsu, H. -W.; Kempf, S.] Univ Boulder, Boulder, CO USA.
[Hillier, J.] Univ Kent, Canterbury CT2 7NZ, Kent, England.
[Blum, J.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany.
[Burton, M.] Jet Prop Lab, Pasadena, CA USA.
RP Altobelli, N (reprint author), European Space Agcy, European Space Astron Ctr, Madrid, Spain.
EM nicolas.altobelli@sciops.esa.int
FU European Space Agency; Deutsche Forschungsgemeinschaft (DFG) [1385, BL
298/20-2, TR333/14, SR77/1]; European Union [622856]; Deutsches Zentrum
fur Luft- und Raumfahrt (DLR), Germany; International Space Science
Institute; DFG; Klaus Tschira Foundation
FX N.A. and F.P. acknowledge European Space Agency faculty funding for
travels and meetings that were necessary for the completion of this
work. Funding through Deutsche Forschungsgemeinschaft (DFG) within the
priority program 1385 "The First 10 Million Years of the Solar System -
A Planetary Materials Approach" is acknowledged by K.F., J.B. (grant BL
298/20-2), and R.S., M.T., E.G., J.H., and F.P. (grants TR333/14 and
SR77/1). J.H. has received funding from the People Programme (Marie
Curie Actions) of the European Union's Seventh Framework Programme FP7
2013 under Reemployment and Eligibility Assessment (REA) grant agreement
number 622856. R.S. and F.P. acknowledge funding through Deutsches
Zentrum fur Luft- und Raumfahrt (DLR), Germany. V.J.S. acknowledges
funding through the International Space Science Institute. N.K.
acknowledges funding through the DFG. M.T. acknowledges funding by the
Klaus Tschira Foundation. We thank J. Leitner, A. Westphal, R. Stroud,
L. Nittler, P. Hoppe, H. Ishii, and H.-P. Gail for helpful discussions.
We thank three anonymous reviewers for their thorough review of this
paper. All CDA data used for this analysis are archived on the Small
Bodies Node of the Planetary Data System (PDS-SBN), at
http://sbn.psi.edu/archive/cocda.
NR 42
TC 8
Z9 8
U1 2
U2 5
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD APR 15
PY 2016
VL 352
IS 6283
BP 312
EP 318
DI 10.1126/science.aac6397
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DJ1UK
UT WOS:000373990100033
PM 27081064
ER
PT J
AU Yu, Y
Zhang, YX
Chen, Y
Xu, ZJ
AF Yu, Yi
Zhang, Youxue
Chen, Yang
Xu, Zhengjiu
TI Kinetics of anorthite dissolution in basaltic melt
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID CONVECTIVE CRYSTAL DISSOLUTION; SILICATE MELTS; MOLTEN SILICATES; QUARTZ
DISSOLUTION; GRANITIC MELTS; MULTICOMPONENT DIFFUSION; PLAGIOCLASE
FELDSPARS; THERMODYNAMIC MODEL; ZIRCON DISSOLUTION; PHASE-RELATIONS
AB We report convection-free anorthite dissolution experiments in a basaltic melt at 1280-1500 degrees C and 0.5 GPa on two different crystallographic surfaces, (1 2 (1) over bar) and ((3) over bar 0 2) to investigate dissolution kinetics. The anisotropy of the anorthite dissolution rate along these two surfaces is negligible. Time series experiments at similar to 1280 degrees C show that anorthite dissolution is mainly controlled by diffusion in the melt within experimental uncertainty. Analytical solutions were used to model the dissolution and diffusion processes, and to obtain the diffusivities and the saturation concentrations of the equilibrium-determining component (Al2O3) for anorthite dissolution into the basaltic melt. For the first time, we are able to show the physical and chemical characteristics of quench growth effect on the near-interface melt using high spatial resolution (0.3 mu m) EDS analyses. For anorthite (An# >= 90) saturation in a melt with 39-53 wt% SiO2 and <= 0.4 wt% H2O, the concentration of Al2O3 in wt% depends on temperature as follows:
ln C-s;Al2O3 = 8.032(+/- 0.192) - 7882(+/- 287)/T,
where T is temperature in K, and errors are given at 1 sigma level. Al2O3 diffusivity in basaltic melt during plagioclase dissolution can be expressed as:
ln D-Al2O3(EBD,plag diss) = -13.69(+/- 1.57) - 19,313(+/- 2485)/T,
where D is in m(2)/s, and the activation energy is 161 +/- 21 kJ/mol. These results are applied to model the convective dissolution of anorthite in basaltic melts. The model indicates that though anorthite crystals can survive for a longer time compared to olivine crystals of the same size in the same melt, the former would rise for a much smaller distance compared to the olivine sinking distance, due to the smaller density contrast between anorthite and melt. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Yu, Yi; Zhang, Youxue; Chen, Yang; Xu, Zhengjiu] Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA.
[Chen, Yang] CALTECH, Jet Prop Lab, M-S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Zhang, YX (reprint author), Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA.
EM youxue@umich.edu
OI Zhang, Youxue/0000-0002-7439-0086
FU United States NSF [EAR-1019440, EAR-1524473, EAR-9911352]; United States
NASA [NNX15AH37G]
FX We thank Pavel Izbekov and Owen Neill for providing the anorthite
crystals, Keith Putirka for providing his collection of literature data
regarding plagioclase-melt equilibrium, and Jeff Kampf for helping with
the single crystal XRD analysis of anorthite crystals. Constructive
formal reviews by Cliff Shaw, Conel Alexander, Mike Toplis, Yan Liang,
and an anonymous reviewer are highly appreciated. Y. Yu thanks Gordon
Moore and Leslie Hayden for training and help on electron microprobe
analyses. This research is supported by United States NSF grants
EAR-1019440 and EAR-1524473 and United States NASA grant NNX15AH37G.
Electron microprobe work is carried out on a Cameca SX100 instrument at
Electron Microbeam Analysis Laboratory of the University of Michigan,
which was supported by United States NSF grant EAR-9911352.
NR 67
TC 3
Z9 3
U1 8
U2 13
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD APR 15
PY 2016
VL 179
BP 257
EP 274
DI 10.1016/j.gca.2016.02.002
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DH1SS
UT WOS:000372565800014
ER
PT J
AU Toomey, E
Xu, J
Vecchioni, S
Rothschild, L
Wind, S
Fernandes, GE
AF Toomey, Emily
Xu, Jimmy
Vecchioni, Simon
Rothschild, Lynn
Wind, Shalom
Fernandes, Gustavo E.
TI Comparison of Canonical versus Silver(I)-Mediated Base-Pairing on Single
Molecule Conductance in Polycytosine dsDNA
SO JOURNAL OF PHYSICAL CHEMISTRY C
LA English
DT Article
ID DNA-MOLECULES; METALLIZATION; TRANSPORT; JUNCTIONS; DUPLEXES
AB Intercalation of metal ions into double-stranded DNA has recently been proposed as a path to efficient charge transport in DNA wires. Until now, the effect of Ag(I) intercalation between mismatched cytosine nucleobases on the conductance of DNA has not been assessed. Here we use a scanning tunneling microscopy (STM) break-junction technique to evaluate and compare the single molecule conductance of polynucleotide sequences of 11 base pairs in length. The resulting single molecule conductance for Ag(I)-polyC is found to be an order of magnitude greater than the control strand made using canonical Watson-Crick pairing. This finding suggests that Ag(I) intercalation alters the dominant electron transport process from standard g-orbital delocalization common in sequences with multiple stacked guanines to an alternate and ultimately more efficient conduit.
C1 [Toomey, Emily; Xu, Jimmy; Fernandes, Gustavo E.] Brown Univ, Sch Engn, Providence, RI 02912 USA.
[Vecchioni, Simon; Wind, Shalom] Columbia Univ, Dept Biomed Engn, New York, NY 10027 USA.
[Rothschild, Lynn] NASA, Ames Res Ctr, Biospher Sci Branch, Moffett Field, CA 94035 USA.
RP Fernandes, GE (reprint author), Brown Univ, Sch Engn, Providence, RI 02912 USA.
EM gustavo_fernandes@brown.edu
FU U.S. Army Research Laboratory (ARL) [W911NF-14-2-0075]; NSF Partnerships
for Innovation: Building Innovation Capacity [1430007]; AOARD [13RSZ086
(134121)]; NASA Ames Research Center Investment Fund; NASA Space
Technology Research Fellowship; Rhode Island Space Grant; Karen T. Romer
Undergraduate Research and "Teaching Award at Brown University"
FX We gratefully acknowledge the support of U.S. Army Research Laboratory
(ARL) Contract W911NF-14-2-0075, the NSF Partnerships for Innovation:
Building Innovation Capacity program award 1430007, AOARD Grant 13RSZ086
(134121), the NASA Ames Research Center Investment Fund, a NASA Space
Technology Research Fellowship to S.V., the Rhode Island Space Grant,
and the Karen T. Romer Undergraduate Research and "Teaching Award at
Brown University." We also acknowledge support from the NSF Partnerships
for Innovation: Building Innovation Capacity program award 1430007 and
from AOARD Grant 13RSZ086 (134121).
NR 22
TC 3
Z9 3
U1 11
U2 15
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1932-7447
J9 J PHYS CHEM C
JI J. Phys. Chem. C
PD APR 14
PY 2016
VL 120
IS 14
BP 7804
EP 7809
DI 10.1021/acs.jpcc.5b11968
PG 6
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA DJ7ZJ
UT WOS:000374431400040
ER
PT J
AU Bera, PP
Nuevo, M
Materese, CK
Sandford, SA
Lee, TJ
AF Bera, Partha P.
Nuevo, Michel
Materese, Christopher K.
Sandford, Scott A.
Lee, Timothy J.
TI Mechanisms for the formation of thymine under astrophysical conditions
and implications for the origin of life
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID POLYCYCLIC AROMATIC-HYDROCARBONS; INTERSTELLAR ICE ANALOGS; FOCK
PERTURBATION-THEORY; CYTOSINE BASE-PAIR; CARBONACEOUS METEORITES;
ULTRAVIOLET PHOTOIRRADIATION; AMINO-ACIDS; EXTRATERRESTRIAL NUCLEOBASES;
PREBIOTIC MOLECULES; MURCHISON METEORITE
AB Nucleobases are the carriers of the genetic information in ribonucleic acid and deoxyribonucleic acid (DNA) for all life on Earth. Their presence in meteorites clearly indicates that compounds of biological importance can form via non-biological processes in extraterrestrial environments. Recent experimental studies have shown that the pyrimidine-based nucleobases uracil and cytosine can be easily formed from the ultraviolet irradiation of pyrimidine in H2O-rich ice mixtures that simulate astrophysical processes. In contrast, thymine, which is found only in DNA, is more difficult to form under the same experimental conditions, as its formation usually requires a higher photon dose. Earlier quantum chemical studies confirmed that the reaction pathways were favorable provided that several H2O molecules surrounded the reactants. However, the present quantum chemical study shows that the formation of thymine is limited because of the inefficiency of the methylation of pyrimidine and its oxidized derivatives in an H2O ice, as supported by the laboratory studies. Our results constrain the formation of thymine in astrophysical environments and thus the inventory of organic molecules delivered to the early Earth and have implications for the role of thymine and DNA in the origin of life. Published by AIP Publishing.
C1 [Bera, Partha P.; Nuevo, Michel; Materese, Christopher K.; Sandford, Scott A.; Lee, Timothy J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Bera, Partha P.; Nuevo, Michel; Materese, Christopher K.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
RP Bera, PP; Lee, TJ (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.; Bera, PP (reprint author), Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
EM Partha.P.Bera@nasa.gov; Timothy.J.Lee@nasa.gov
RI Lee, Timothy/K-2838-2012
FU National Aeronautics and Space Administration through the NASA
Astrobiology Institute [NNH13ZDA017C]; NASA consortium "Carbon in the
galaxy" grant
FX Part of this material is based upon work supported by the National
Aeronautics and Space Administration through the NASA Astrobiology
Institute under Cooperative Agreement Notice No. NNH13ZDA017C issued
through the Science Mission Directorate. The NASA "Origins of Solar
Systems" program, the NASA consortium "Carbon in the galaxy" grant, and
the NASA Postdoctoral Programs are gratefully acknowledged. M.N.,
C.K.M., and S.A.S. would like to acknowledge Robert L. Walker (NASA
Ames) for technical support.
NR 51
TC 2
Z9 2
U1 10
U2 20
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-9606
EI 1089-7690
J9 J CHEM PHYS
JI J. Chem. Phys.
PD APR 14
PY 2016
VL 144
IS 14
AR 144308
DI 10.1063/1.4945745
PG 7
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DK2WB
UT WOS:000374774000023
PM 27083722
ER
PT J
AU Demory, BO
Gillon, M
de Wit, J
Madhusudhan, N
Bolmont, E
Heng, K
Kataria, T
Lewis, N
Hu, RY
Krick, J
Stamenkovic, V
Benneke, B
Kane, S
Queloz, D
AF Demory, Brice-Olivier
Gillon, Michael
de Wit, Julien
Madhusudhan, Nikku
Bolmont, Emeline
Heng, Kevin
Kataria, Tiffany
Lewis, Nikole
Hu, Renyu
Krick, Jessica
Stamenkovic, Vlada
Benneke, Bjorn
Kane, Stephen
Queloz, Didier
TI A map of the large day-night temperature gradient of a super-Earth
exoplanet
SO NATURE
LA English
DT Article
ID 55 CANCRI E; HD 189733B; WARM SPITZER; PLANET; ATMOSPHERES; TRANSIT;
STAR; ECLIPSES; VARIABILITY; INFERENCE
AB Over the past decade, observations of giant exoplanets (Jupiter-size) have provided key insights into their atmospheres(1,2), but the properties of lower-mass exoplanets (sub-Neptune) remain largely unconstrained because of the challenges of observing small planets. Numerous efforts to observe the spectra of super-Earths-exoplanets with masses of one to ten times that of Earth-have so far revealed only featureless spectra(3). Here we report a longitudinal thermal brightness map of the nearby transiting super-Earth 55 Cancri e (refs 4, 5) revealing highly asymmetric dayside thermal emission and a strong day-night temperature contrast. Dedicated space-based monitoring of the planet in the infrared revealed a modulation of the thermal flux as 55 Cancri e revolves around its star in a tidally locked configuration. These observations reveal a hot spot that is located 41 +/- 12 degrees east of the substellar point (the point at which incident light from the star is perpendicular to the surface of the planet). From the orbital phase curve, we also constrain the nightside brightness temperature of the planet to 1,380 +/- 400 kelvin and the temperature of the warmest hemisphere (centred on the hot spot) to be about 1,300 kelvin hotter (2,700 +/- 270 kelvin) at a wavelength of 4.5 micrometres, which indicates inefficient heat redistribution from the dayside to the nightside. Our observations are consistent with either an optically thick atmosphere with heat recirculation confined to the planetary dayside, or a planet devoid of atmosphere with low-viscosity magma flows at the surface(6).
C1 [Demory, Brice-Olivier; Queloz, Didier] Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England.
[Gillon, Michael] Univ Liege, Inst Astrophys & Geophys, Allee 6 Aout 17, B-4000 Liege, Belgium.
[de Wit, Julien] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Bolmont, Emeline] Univ Namur, Dept Math, NaXys, 8 Rempart Vierge, B-5000 Namur, Belgium.
[Heng, Kevin] Univ Bern, Ctr Space & Habitabil, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Kataria, Tiffany] Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England.
[Lewis, Nikole] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Hu, Renyu; Stamenkovic, Vlada] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Hu, Renyu; Stamenkovic, Vlada; Benneke, Bjorn] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Krick, Jessica] CALTECH, Jet Prop Lab, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA.
[Kane, Stephen] San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA.
RP Demory, BO (reprint author), Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England.
EM bod21@cam.ac.uk
OI Stamenkovic, Vlada/0000-0003-2416-3683; Demory,
Brice-Olivier/0000-0002-9355-5165
FU NASA; Simons Foundation [338555]
FX We thank D. Deming, D. Apai and A. Showman for discussions as well as
the Spitzer Science Center staff for their assistance in the planning
and executing of these observations. This work is based on observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA. Support for this work was provided by NASA through
an award issued by JPL/Caltech. M.G. is a Research Associate at the
Belgian Funds for Scientific Research (FRS-FNRS). V.S. was supported by
the Simons Foundation (award number 338555, VS).
NR 46
TC 9
Z9 9
U1 9
U2 17
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD APR 14
PY 2016
VL 532
IS 7598
BP 207
EP +
DI 10.1038/nature17169
PG 16
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DJ7TJ
UT WOS:000374415100033
PM 27027283
ER
PT J
AU Ackermann, M
Ajello, M
Albert, A
Atwood, WB
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Bissaldi, E
Blandford, RD
Bloom, ED
Bonino, R
Bregeon, J
Britto, RJ
Bruel, P
Buehler, R
Caliandro, GA
Cameron, RA
Caragiulo, M
Caraveo, PA
Cavazzuti, E
Cecchi, C
Charles, E
Chekhtman, A
Chiang, J
Chiaro, G
Ciprini, S
Cohen-Tanugi, J
Cominsky, LR
Costanza, F
Cutini, S
D'Ammando, F
de Angelis, A
de Palma, F
Desiante, R
Digel, SW
Di Mauro, M
Di Venere, L
Dominguez, A
Drell, PS
Favuzzi, C
Fegan, SJ
Ferrara, EC
Franckowiak, A
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Godfrey, G
Green, D
Grenier, IA
Guiriec, S
Hays, E
Horan, D
Iafrate, G
Jogler, T
Johannesson, G
Kuss, M
La Mura, G
Larsson, S
Latronico, L
Li, J
Li, L
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Magill, J
Maldera, S
Manfreda, A
Mayer, M
Mazziotta, MN
Michelson, PF
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Negro, M
Nuss, E
Ohsugi, T
Okada, C
Omodei, N
Orlando, E
Ormes, JF
Paneque, D
Perkins, JS
Pesce-Rollins, M
Petrosian, V
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Reposeur, T
Romani, RW
Sanchez-Conde, M
Schmid, J
Schulz, A
Sgro, C
Simone, D
Siskind, EJ
Spada, F
Spandre, G
Spinelli, P
Suson, DJ
Takahashi, H
Thayer, JB
Tibaldo, L
Torres, DF
Troja, E
Vianello, G
Yassine, M
Zimmer, S
AF Ackermann, M.
Ajello, M.
Albert, A.
Atwood, W. B.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bloom, E. D.
Bonino, R.
Bregeon, J.
Britto, R. J.
Bruel, P.
Buehler, R.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Caraveo, P. A.
Cavazzuti, E.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiang, J.
Chiaro, G.
Ciprini, S.
Cohen-Tanugi, J.
Cominsky, L. R.
Costanza, F.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Desiante, R.
Digel, S. W.
Di Mauro, M.
Di Venere, L.
Dominguez, A.
Drell, P. S.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Franckowiak, A.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Godfrey, G.
Green, D.
Grenier, I. A.
Guiriec, S.
Hays, E.
Horan, D.
Iafrate, G.
Jogler, T.
Johannesson, G.
Kuss, M.
La Mura, G.
Larsson, S.
Latronico, L.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Magill, J.
Maldera, S.
Manfreda, A.
Mayer, M.
Mazziotta, M. N.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Moiseev, A. A.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Negro, M.
Nuss, E.
Ohsugi, T.
Okada, C.
Omodei, N.
Orlando, E.
Ormes, J. F.
Paneque, D.
Perkins, J. S.
Pesce-Rollins, M.
Petrosian, V.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Reposeur, T.
Romani, R. W.
Sanchez-Conde, M.
Schmid, J.
Schulz, A.
Sgro, C.
Simone, D.
Siskind, E. J.
Spada, F.
Spandre, G.
Spinelli, P.
Suson, D. J.
Takahashi, H.
Thayer, J. B.
Tibaldo, L.
Torres, D. F.
Troja, E.
Vianello, G.
Yassine, M.
Zimmer, S.
TI Resolving the Extragalactic gamma-Ray Background above 50 GeV with the
Fermi Large Area Telescope
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID X-RAY; STATISTICS; EMISSION; SPECTRUM; BLAZARS; ORIGIN; HOLE
AB The Fermi Large Area Telescope (LAT) Collaboration has recently released a catalog of 360 sources detected above 50 GeV (2FHL). This catalog was obtained using 80 months of data re-processed with Pass 8, the newest event-level analysis, which significantly improves the acceptance and angular resolution of the instrument. Most of the 2FHL sources at high Galactic latitude are blazars. Using detailed Monte Carlo simulations, we measure, for the first time, the source count distribution, dN= dS, of extragalactic.-ray sources at E > 50 GeV and find that it is compatible with a Euclidean distribution down to the lowest measured source flux in the 2FHL (8 x 10(-12) ph cm(-2) s(-1)). We employ a one-point photon fluctuation analysis to constrain the behavior of dN= dS below the source detection threshold. Overall, the source count distribution is constrained over three decades in flux and found compatible with a broken power law with a break flux, Sb, in the range [8 x 10-12; 1.5 x 10-11] ph cm(-2) s(-1) and power-law indices below and above the break of a 2. [1.60; 1.75] and a 1 +/- 2.49 +/- 0.12, respectively. Integration of dN= dS shows that point sources account for at least 86_16 -14 % of the total extragalactic gamma-ray background. The simple form of the derived source count distribution is consistent with a single population (i. e., blazars) dominating the source counts to the minimum flux explored by this analysis. We estimate the density of sources detectable in blind surveys that will be performed in the coming years by the Cherenkov Telescope Array.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.; Dominguez, A.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Albert, A.; Baldini, L.; Blandford, R. D.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Digel, S. W.; Di Mauro, M.; Drell, P. S.; Franckowiak, A.; Godfrey, G.; Jogler, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Thayer, J. B.; Vianello, G.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Albert, A.; Baldini, L.; Blandford, R. D.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Digel, S. W.; Di Mauro, M.; Drell, P. S.; Franckowiak, A.; Godfrey, G.; Jogler, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Thayer, J. B.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Atwood, W. B.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Grenier, I. A.; Schmid, J.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Iafrate, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Chiaro, G.; La Mura, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bechtol, K.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
[Bechtol, K.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Bellazzini, R.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bissaldi, E.; Caragiulo, M.; Costanza, F.; de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Simone, D.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bonino, R.; Desiante, R.; Latronico, L.; Maldera, S.; Negro, M.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bonino, R.; Negro, M.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Yassine, M.] Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, F-34059 Montpellier, France.
[Britto, R. J.; Razzaque, S.] Univ Johannesburg, Dept Phys, POB 524, ZA-2006 Auckland Pk, South Africa.
[Bruel, P.; Fegan, S. J.; Horan, D.] CNRS IN2P3, Ecole Polytech, Lab Leprince Ringuet, Palaiseau, France.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy.
[Cecchi, C.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA.
[Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA.
[Cutini, S.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy.
[D'Ammando, F.; Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Grp Collegato Udine, Sez Trieste, Ist Nazl Fis Nucl, I-33100 Udine, Italy.
[de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Ferrara, E. C.; Green, D.; Guiriec, S.; Hays, E.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fukazawa, Y.; Okada, C.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Funk, S.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Green, D.; Magill, J.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Green, D.; Magill, J.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Guiriec, S.] NASA, Postdoctoral Program, New York, NY USA.
[Iafrate, G.] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy.
[Johannesson, G.] Univ Iceland, Inst Sci, Dunhaga 3, IS-107 Reykjavik, Iceland.
[La Mura, G.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[La Mura, G.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Physik, A-6020 Innsbruck, Austria.
[Larsson, S.; Li, L.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Larsson, S.; Li, L.; Sanchez-Conde, M.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Li, J.; Torres, D. F.] Inst Space Sci IEEC CSIC, Campus UAB, E-08193 Barcelona, Spain.
[Lott, B.; Reposeur, T.] Univ Bordeaux 1, Ctr Etudes Nucl Bordeaux Gradignan, IN2P3 CNRS, BP120, F-33175 Gradignan, France.
[Lovellette, M. N.] Naval Res Lab, Space Sci Div, Washington, DC 20375 USA.
[Mitthumsiri, W.] Mahidol Univ, Dept Phys, Fac Sci, Bangkok 10400, Thailand.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA.
[Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Murgia, S.] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Sanchez-Conde, M.; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Tibaldo, L.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Torres, D. F.] ICREA, Barcelona, Spain.
RP Ajello, M (reprint author), Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.; Di Mauro, M (reprint author), Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.; Di Mauro, M (reprint author), Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
EM majello@slac.stanford.edu; mattia.dimauro@to.infn.it
RI Moskalenko, Igor/A-1301-2007; Bissaldi, Elisabetta/K-7911-2016; Reimer,
Olaf/A-3117-2013; Orlando, E/R-5594-2016; Funk, Stefan/B-7629-2015;
Bonino, Raffaella/S-2367-2016; Torres, Diego/O-9422-2016; Di Venere,
Leonardo/C-7619-2017;
OI Moskalenko, Igor/0000-0001-6141-458X; Bissaldi,
Elisabetta/0000-0001-9935-8106; Reimer, Olaf/0000-0001-6953-1385; Funk,
Stefan/0000-0002-2012-0080; Torres, Diego/0000-0002-1522-9065; Di
Venere, Leonardo/0000-0003-0703-824X; Sgro', Carmelo/0000-0001-5676-6214
NR 28
TC 12
Z9 12
U1 4
U2 18
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 14
PY 2016
VL 116
IS 15
AR 151105
DI 10.1103/PhysRevLett.116.151105
PG 8
WC Physics, Multidisciplinary
SC Physics
GA DJ1SN
UT WOS:000373984100003
PM 27127954
ER
PT J
AU Long, D
Chen, X
Scanlon, BR
Wada, Y
Hong, Y
Singh, VP
Chen, YN
Wang, CG
Han, ZY
Yang, WT
AF Long, Di
Chen, Xi
Scanlon, Bridget R.
Wada, Yoshihide
Hong, Yang
Singh, Vijay P.
Chen, Yaning
Wang, Cunguang
Han, Zhongying
Yang, Wenting
TI Have GRACE satellites overestimated groundwater depletion in the
Northwest India Aquifer?
SO SCIENTIFIC REPORTS
LA English
DT Article
ID GLOBAL HYDROLOGICAL MODEL; WATER STORAGE; GRAVITY MEASUREMENTS;
MIDDLE-EAST; STRESS; AVAILABILITY; VARIABILITY; IRRIGATION; DROUGHT;
SYSTEM
AB The Northwest India Aquifer (NWIA) has been shown to have the highest groundwater depletion (GWD) rate globally, threatening crop production and sustainability of groundwater resources. Gravity Recovery and Climate Experiment (GRACE) satellites have been emerging as a powerful tool to evaluate GWD with ancillary data. Accurate GWD estimation is, however, challenging because of uncertainties in GRACE data processing. We evaluated GWD rates over the NWIA using a variety of approaches, including newly developed constrained forward modeling resulting in a GWD rate of 3.1 +/- 0.1 cm/a (or 14 +/- 0.4 km(3)/a) for Jan 2005-Dec 2010, consistent with the GWD rate (2.8 cm/a or 12.3 km(3)/a) from groundwater-level monitoring data. Published studies (e.g., 4 +/- 1 cm/a or 18 +/- 4.4 km(3)/a) may overestimate GWD over this region. This study highlights uncertainties in GWD estimates and the importance of incorporating a priori information to refine spatial patterns of GRACE signals that could be more useful in groundwater resource management and need to be paid more attention in future studies.
C1 [Long, Di; Chen, Xi; Hong, Yang; Wang, Cunguang; Han, Zhongying; Yang, Wenting] Tsinghua Univ, Dept Hydraul Engn, State Key Lab Hydrosci & Engn, Beijing 100084, Peoples R China.
[Scanlon, Bridget R.] Univ Texas Austin, Jackson Sch Geosci, Bur Econ Geol, Austin, TX 78758 USA.
[Wada, Yoshihide] Univ Utrecht, Dept Phys Geog, Utrecht, Netherlands.
[Wada, Yoshihide] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Wada, Yoshihide] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Wada, Yoshihide] Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria.
[Hong, Yang] Univ Oklahoma, Dept Civil Engn & Environm Sci, Norman, OK 73072 USA.
[Singh, Vijay P.] Texas A&M Univ, Dept Biol & Agr Engn, College Stn, TX 77843 USA.
[Singh, Vijay P.] Texas A&M Univ, Dept Civil & Environm Engn, College Stn, TX 77843 USA.
[Chen, Yaning] Chinese Acad Sci, Xinjiang Inst Ecol & Geog, State Key Lab Desert & Oasis Ecol, Urumqi 830011, Xinjiang, Peoples R China.
RP Long, D (reprint author), Tsinghua Univ, Dept Hydraul Engn, State Key Lab Hydrosci & Engn, Beijing 100084, Peoples R China.
EM dlong@tsinghua.edu.cn
RI Long, Di/N-8049-2013; Scanlon, Bridget/A-3105-2009; Hong,
Yang/D-5132-2009
OI Long, Di/0000-0001-9033-5039; Scanlon, Bridget/0000-0002-1234-4199;
Hong, Yang/0000-0001-8720-242X
FU National Natural Science Foundation of China [91547210, 91437214,
51579128]
FX We are grateful to Dr. Jianli Chen's help with illustrating forward
modeling techniques, Dr. Laurent Longuevergne for illustrating the
additive and multiplicative correction approaches, and Dr. Petra Doll
for providing the WGHM output for this analysis. CSR RL05 Level 2 data
are available at the Center for Space Research at the University of
Texas at Austin; gridded scaling factors from CLM4.0 are available at
the Jet Propulsion Laboratory, California Institute of Technology; and
GLDAS-1 output is available at the Goddard Earth Sciences Data and
Information Services Center, NASA. We'd also like to thank India's
Central Ground Water Board (CGWB) for providing groundwater-level
monitoring data in districts of the three-state region and its
surroundings for the period 2005-2010 through the Groundwater
Information System hosted by the National Informatics Centre. This study
was jointly supported by the National Natural Science Foundation of
China (Grant No. 91547210, 91437214 and 51579128).
NR 43
TC 6
Z9 6
U1 6
U2 19
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD APR 14
PY 2016
VL 6
AR 24398
DI 10.1038/srep24398
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DJ2ME
UT WOS:000374038000001
PM 27075595
ER
PT J
AU Dubernet, ML
Antony, BK
Ba, YA
Babikov, YL
Bartschat, K
Boudon, V
Braams, BJ
Chung, HK
Daniel, F
Delahaye, F
Del Zanna, G
de Urquijo, J
Dimitrijevic, MS
Domaracka, A
Doronin, M
Drouin, BJ
Endres, CP
Fazliev, AZ
Gagarin, SV
Gordon, IE
Gratier, P
Heiter, U
Hill, C
Jevremovic, D
Joblin, C
Kasprzak, A
Krishnakumar, E
Leto, G
Loboda, PA
Louge, T
Maclot, S
Marinkovic, BP
Markwick, A
Marquart, T
Mason, HE
Mason, NJ
Mendoza, C
Mihajlov, AA
Millar, TJ
Moreau, N
Mulas, G
Pakhomov, Y
Palmeri, P
Pancheshnyi, S
Perevalov, VI
Piskunov, N
Postler, J
Quinet, P
Quintas-Sanchez, E
Ralchenko, Y
Rhee, YJ
Rixon, G
Rothman, LS
Roueff, E
Ryabchikova, T
Sahal-Brechot, S
Scheier, P
Schlemmer, S
Schmitt, B
Stempels, E
Tashkun, S
Tennyson, J
Tyuterev, VG
Vujcic, V
Wakelam, V
Walton, NA
Zatsarinny, O
Zeippen, CJ
Zwolf, CM
AF Dubernet, M. L.
Antony, B. K.
Ba, Y. A.
Babikov, Yu L.
Bartschat, K.
Boudon, V.
Braams, B. J.
Chung, H-K
Daniel, F.
Delahaye, F.
Del Zanna, G.
de Urquijo, J.
Dimitrijevic, M. S.
Domaracka, A.
Doronin, M.
Drouin, B. J.
Endres, C. P.
Fazliev, A. Z.
Gagarin, S. V.
Gordon, I. E.
Gratier, P.
Heiter, U.
Hill, C.
Jevremovic, D.
Joblin, C.
Kasprzak, A.
Krishnakumar, E.
Leto, G.
Loboda, P. A.
Louge, T.
Maclot, S.
Marinkovic, B. P.
Markwick, A.
Marquart, T.
Mason, H. E.
Mason, N. J.
Mendoza, C.
Mihajlov, A. A.
Millar, T. J.
Moreau, N.
Mulas, G.
Pakhomov, Yu
Palmeri, P.
Pancheshnyi, S.
Perevalov, V. I.
Piskunov, N.
Postler, J.
Quinet, P.
Quintas-Sanchez, E.
Ralchenko, Yu
Rhee, Y-J
Rixon, G.
Rothman, L. S.
Roueff, E.
Ryabchikova, T.
Sahal-Brechot, S.
Scheier, P.
Schlemmer, S.
Schmitt, B.
Stempels, E.
Tashkun, S.
Tennyson, J.
Tyuterev, Vl G.
Vujcic, V.
Wakelam, V.
Walton, N. A.
Zatsarinny, O.
Zeippen, C. J.
Zwoelf, C. M.
TI The virtual atomic and molecular data centre (VAMDC) consortium
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Article
DE databases; atoms; molecules; spectroscopy; kinetic data; astrophysics
ID LOW-ENERGY-ELECTRON; LINE-DATA-BASE; IRRADIATION EXPERIMENTS RELEVANT;
STIMULATED RAMAN-SPECTROSCOPY; HIGH-RESOLUTION SPECTROSCOPY; R-MATRIX
METHOD; CW-CAVITY RING; ION IRRADIATION; CROSS-SECTIONS; COLLISIONAL
DATABASE
AB The Virtual Atomic and Molecular Data Centre (VAMDC) Consortium is a worldwide consortium which federates atomic and molecular databases through an e-science infrastructure and an organisation to support this activity. About 90% of the inter-connected databases handle data that are used for the interpretation of astronomical spectra and for modelling in many fields of astrophysics. Recently the VAMDC Consortium has connected databases from the radiation damage and the plasma communities, as well as promoting the publication of data from Indian institutes. This paper describes how the VAMDC Consortium is organised for the optimal distribution of atomic and molecular data for scientific research. It is noted that the VAMDC Consortium strongly advocates that authors of research papers using data cite the original experimental and theoretical papers as well as the relevant databases.
C1 [Dubernet, M. L.; Ba, Y. A.; Delahaye, F.; Dimitrijevic, M. S.; Doronin, M.; Moreau, N.; Quintas-Sanchez, E.; Roueff, E.; Sahal-Brechot, S.; Zeippen, C. J.; Zwoelf, C. M.] Univ Paris 06, Univ Sorbonne, CNRS, LERMA,Observ Paris,PSL Res Univ, 5 Pl Janssen, F-92190 Meudon, France.
[Antony, B. K.] Indian Sch Mines, Dept Appl Phys, Dhanbad 826004, Bihar, India.
[Babikov, Yu L.; Fazliev, A. Z.; Perevalov, V. I.; Tashkun, S.] Russian Acad Sci, Inst Atmospher Opt, Zuev Sq 1, Tomsk 634021, Russia.
[Babikov, Yu L.] Tomsk State Univ, Tomsk 634050, Russia.
[Bartschat, K.; Zatsarinny, O.] Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA.
[Boudon, V.] Univ Bourgogne Franche Comte, CNRS, UMR 6303, Lab Interdisciplinaire Carnot Bourgogne, 9 Ave Alain Savary,BP 47 870, F-21078 Dijon, France.
[Braams, B. J.; Chung, H-K] IAEA, Vienna Int Ctr, Div Phys & Chem Sci, Nucl Data Sect, A-1400 Vienna, Austria.
[Daniel, F.; Schmitt, B.] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France.
[Del Zanna, G.; Mason, H. E.] Ctr Math Sci, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England.
[de Urquijo, J.] Univ Nacl Autonoma Mexico, Inst Ciencias Fis, POB 48-3, Cuernavaca 62251, Morelos, Mexico.
[Dimitrijevic, M. S.; Jevremovic, D.; Vujcic, V.] Astron Observ, Volgina 7, Belgrade 11060, Serbia.
[Domaracka, A.; Maclot, S.] UCN, ENSICAEN, CNRS, CIMAP,UMR 6252,CEA, Bd Henri Becquerel,BP 5133, F-14070 Caen 5, France.
[Drouin, B. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Endres, C. P.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Gagarin, S. V.; Loboda, P. A.] Russian Fed Nucl Ctr All Russian Inst Tech Phys R, Snezhinsk, Russia.
[Gordon, I. E.; Rothman, L. S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, MS50,60 Garden St, Cambridge, MA 02138 USA.
[Gratier, P.; Wakelam, V.] Univ Bordeaux, LAB, UMR 5804, F-33270 Florac, France.
[Gratier, P.; Wakelam, V.] CNRS, LAB, UMR 5804, F-33270 Florac, France.
[Heiter, U.; Marquart, T.; Piskunov, N.; Stempels, E.] Uppsala Univ, Dept Phys & Astron, Box 516, SE-75120 Uppsala, Sweden.
[Hill, C.; Tennyson, J.] UCL, Dept Phys & Astron, Mortimer St, London WC1E 6BT, England.
[Joblin, C.; Louge, T.; Mulas, G.] Univ Toulouse, UPS OMP, CNRS, Inst Rech Astrophys & Planetol, 9 Av Colonel Roche, F-31028 Toulouse 4, France.
[Kasprzak, A.] Observ Paris, SRCV, 61 Av Denfert Rochereau, F-75014 Paris, France.
[Krishnakumar, E.] Tata Inst Fundamental Res, Dept Nucl & Atom Phys, Homi Bhabha Rd, Bombay 400005, Maharashtra, India.
[Leto, G.] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy.
[Loboda, P. A.] Natl Res Nucl Univ, Moscow Engn Phys Inst MEPhI, Moscow, Russia.
[Maclot, S.] Univ Caen Normandie, Esplanade Paix, CS 14032, F-14032 Caen 5, France.
[Marinkovic, B. P.; Mihajlov, A. A.] Univ Belgrade, Inst Phys Belgrade, POB 57, Belgrade 11001, Serbia.
[Markwick, A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England.
[Mason, N. J.] Open Univ, Dept Phys Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
[Mendoza, C.] IVIC, Ctr Fis, POB 20632, Caracas 1020A, Venezuela.
[Millar, T. J.] Queens Univ Belfast, Sch Math & Phys, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland.
[Mulas, G.] Osservatorio Astron Cagliari, Ist Nazl AstroFis, Via Sci 5, I-09047 Selargius, CA, Italy.
[Pakhomov, Yu; Ryabchikova, T.] RAS, Inst Astron, Pyatnitskaya 48, Moscow 119017, Russia.
[Palmeri, P.; Quinet, P.] Univ Mons, Phys Atom & Astrophys, B-7000 Mons, Belgium.
[Pancheshnyi, S.] ABB Corp Res, Segelhofstr 1K, CH-5405 Baden, Switzerland.
[Postler, J.; Scheier, P.] Univ Innsbruck, Inst Ion Phys & Appl Phys, Technikerstr 25-3, A-6020 Innsbruck, Austria.
[Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium.
[Ralchenko, Yu] NIST, Atom Spect Grp, Gaithersburg, MD 20899 USA.
[Rhee, Y-J] Korea Atom Energy Res Inst, Nucl Data Ctr, Taejon 305353, South Korea.
[Rixon, G.; Walton, N. A.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Schlemmer, S.] Univ Cologne, Inst Phys 1, zulpicher Str 77, D-50937 Kln, Germany.
[Tyuterev, Vl G.] Univ Reims, GSMA, UMR CNRS 7331, Reims, France.
[Vujcic, V.] Univ Belgrade, Fac Org Sci, Jove Ilica 33, Belgrade 11000, Serbia.
RP Dubernet, ML (reprint author), Univ Paris 06, Univ Sorbonne, CNRS, LERMA,Observ Paris,PSL Res Univ, 5 Pl Janssen, F-92190 Meudon, France.
EM marie-lise.dubernet@obspm.fr
RI Tennyson, Jonathan/I-2222-2012; Scheier, Paul/E-3088-2010; Tashkun,
Sergey/E-8682-2014; Marinkovic, Bratislav/D-3589-2012; Babikov,
Yurii/E-8686-2014; Antony, Bobby Kachappilly/H-5302-2015; Pakhomov,
Yury/B-5172-2014;
OI Tennyson, Jonathan/0000-0002-4994-5238; Marinkovic,
Bratislav/0000-0002-6904-6360; Antony, Bobby
Kachappilly/0000-0003-2073-9681; Leto, Giuseppe/0000-0002-0040-5011;
Wakelam, Valentine/0000-0001-9676-2605; Mulas,
Giacomo/0000-0003-0602-6669; Millar, Tom/0000-0001-5178-3656
FU VAMDC project; SUP@VAMDC project [INFRA-2008-1.2.2, 239108, 313284];
Paris Astronomical Data Center; UK Science and Technology Facilities
Council (STFC) [ST/M007731/1, ST/M007774/1, ST/M007766/1]; NASA; UK
STFC; SOLID (First European SOLar Irradiance Data Exploitation), a
collaborative SPACE Project under the Seventh Framework Programme (FP7)
of the European Commission [313188]; Russian Foundation for Basic
Research, RFBR grant [14-07-00863]; NASA Planetary Atmospheres Grant
[NNX13AI59G]; ERC Advanced Investigator Project [267219]; United States
National Science Foundation [PHY-1403245, PHY-1520970]; Dept. of Science
and Technology (DST), Govt. of India; Austrian Science Fund (FWF)
[P26635]; Nano-IBCT COST Action MP1002 (Nano-scale Insights into Ion
Beam Cancer Therapy); LIA SAMIA; Tomsk State University D Mendeleev
funding program; Ministry of Education, Science and Technological
Development of Republic of Serbia [III44002, 176002, 171020]; XSEDE
supercomputer allocation [PHY-090031]
FX Support for VAMDC has been provided through the VAMDC and the SUP@VAMDC
projects funded under the 'Combination of Collaborative Projects and
Coordination and Support Actions' Funding Scheme of The Seventh
Framework Program. Call topic: INFRA-2008-1.2.2 and INFRA-2012
Scientific Data Infrastructure. Grant Agreement numbers: 239108 and
313284. In addition we acknowledge support from Paris Astronomical Data
Center. The UK nodes acknowledge support from the UK Science and
Technology Facilities Council (STFC) under grants ST/M007731/1,
ST/M007774/1 and ST/M007766/1. Portions of the research described in
this paper were performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. The NIST ASD development is supported in part
by NASA. GDZ and HEM work on CHIANTI has been supported by the UK STFC
and SOLID (First European SOLar Irradiance Data Exploitation), a
collaborative SPACE Project under the Seventh Framework Programme
(FP7/2007-2013) of the European Commission under Grant Agreement N
313188. The Spectr-W3 project activities are currently
supported in part by the Russian Foundation for Basic Research, RFBR
grant Nr. 14-07-00863. LSR and IEG wish to thank the support from NASA
Planetary Atmospheres Grant NNX13AI59G. ExoMol is supported by ERC
Advanced Investigator Project 267219. ZB and KB acknowledge support from
the United States National Science Foundation under grants PHY-1403245
and PHY-1520970, and by the XSEDE supercomputer allocation PHY-090031.
AD and SM thank P Rousseau and B A Huber for fruitful discussions,
Quentin Marie for the preparing of the RADAM-ION database website
structure and Universite de Caen Normandie for hosting the website. BA
is supported by the Dept. of Science and Technology (DST), Govt. of
India. Part of this research was supported by the Austrian Science Fund
(FWF): P26635. Support from Nano-IBCT COST Action MP1002 (Nano-scale
Insights into Ion Beam Cancer Therapy) is also acknowledged. YLB and VGT
acknowledge support from LIA SAMIA and from Tomsk State University D
Mendeleev funding program. Belgrade node activities and the
corresponding research are supported by projects III44002, 176002 and
171020 of the Ministry of Education, Science and Technological
Development of Republic of Serbia.
NR 162
TC 10
Z9 10
U1 10
U2 29
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
EI 1361-6455
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD APR 14
PY 2016
VL 49
IS 7
AR 074003
DI 10.1088/0953-4075/49/7/074003
PG 18
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA DH6OS
UT WOS:000372911000003
ER
PT J
AU Young, PR
Dere, KP
Landi, E
Del Zanna, G
Mason, HE
AF Young, P. R.
Dere, K. P.
Landi, E.
Del Zanna, G.
Mason, H. E.
TI The CHIANTI atomic database
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Article
DE astrophysics; the Sun; database; atomic physics
ID FINITE-DENSITY PLASMAS; DIELECTRONIC RECOMBINATION DATA; ELECTRON-ION
RECOMBINATION; MAXWELLIAN KAPPA-DISTRIBUTIONS; ULTRAVIOLET
EMISSION-LINES; EUV IMAGING SPECTROMETER; CHARGE-STATE EVOLUTION;
OPTICALLY THIN PLASMAS; HELIUM-LIKE IONS; FAST SOLAR-WIND
AB The freely available CHIANTI atomic database was first released in 1996 and has had a huge impact on the analysis and modeling of emissions from astrophysical plasmas. It contains data and software for modeling optically thin atom and positive ion emission from low density (less than or similar to 10(13) cm(-3)) plasmas from x-ray to infrared wavelengths. A key feature is that the data are assessed and regularly updated, with version 8 released in 2015. Atomic data for modeling the emissivities of 246 ions and neutrals are contained in CHIANTI, together with data for deriving the ionization fractions of all elements up to zinc. The different types of atomic data are summarized here and their formats discussed. Statistics on the impact of CHIANTI to the astrophysical community are given and examples of the diverse range of applications are presented.
C1 [Young, P. R.; Dere, K. P.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Young, P. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Landi, E.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Del Zanna, G.; Mason, H. E.] Univ Cambridge, Ctr Math Sci, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England.
RP Young, PR (reprint author), George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.; Young, PR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM pyoung9@gmu.edu
FU NASA [NNX15AF25G]; UK STFC; SOLID (First European SOLar Irradiance Data
Exploitation), a collaborative SPACE Project under the Seventh Framework
Programme (FP7) of the European Commission [313188]
FX PRY, EL and KPD acknowledge support from NASA grant NNX15AF25G. GDZ and
HEM acknowledge support by the UK STFC and SOLID (First European SOLar
Irradiance Data Exploitation), a collaborative SPACE Project under the
Seventh Framework Programme (FP7/2007-2013) of the European Commission
under Grant Agreement No. 313188. Dr Hardi Peter is thanked for
providing figure 8 and text for section 7.3. This research has made use
of NASA's Astro-physics Data System Bibliographic Services.
NR 93
TC 1
Z9 1
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
EI 1361-6455
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD APR 14
PY 2016
VL 49
IS 7
AR 074009
DI 10.1088/0953-4075/49/7/074009
PG 14
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA DH6OS
UT WOS:000372911000009
ER
PT J
AU Williams, TS
Orloff, ND
Baker, JS
Miller, SG
Natarajan, B
Obrzut, J
McCorkle, LS
Lebron-Colon, M
Gaier, J
Meador, MA
Liddle, JA
AF Williams, Tiffany S.
Orloff, Nathan D.
Baker, James S.
Miller, Sandi G.
Natarajan, Bharath
Obrzut, Jan
McCorkle, Linda S.
Lebron-Colon, Marisabel
Gaier, James
Meador, Michael A.
Liddle, J. Alexander
TI Trade-off between the Mechanical Strength and Microwave Electrical
Properties of Functionalized and Irradiated Carbon Nanotube Sheets
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE multiwalled carbon nanotubes; carbon nanotube sheets; chemical
functionalization; tensile strength; electrical conductivity; microwave
spectroscopy; electron beam irradiation
ID SHEET/BISMALEIMIDE NANOCOMPOSITES; HIGH-PERFORMANCE; CONDUCTIVITY;
BUNDLES; COMPOSITES; FIBERS; YARNS; BEAM
AB Carbon nanotube (CNT) sheets represent a novel implementation of CNTs that enable the tailoring of electrical and mechanical properties for applications in the automotive and aerospace industries. Small molecule functionalization and postprocessing techniques, such as irradiation with high-energy particles, are methods that can enhance the mechanical properties of CNTs. However, the effect that these modifications have on the electrical conduction mechanisms has not been extensively explored. By characterizing the mechanical and electrical properties of multiwalled carbon nanotube (MWCNT) sheets with different functional groups and irradiation doses, we can expand our insights into the extent of the trade-off that exists between mechanical strength and electrical conductivity for commercially available CNT sheets. Such insights allow for the optimization of design pathways for engineering applications that require a balance of material property enhancements.
C1 [Williams, Tiffany S.; Miller, Sandi G.; Lebron-Colon, Marisabel; Gaier, James; Meador, Michael A.] NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA.
[Orloff, Nathan D.; Obrzut, Jan] NIST, Mat Measurement Lab, Gaithersburg, MD 20899 USA.
[Orloff, Nathan D.; Liddle, J. Alexander] NIST, Commun Technol Lab, Boulder, CO 80305 USA.
[Baker, James S.] NASA, Postdoctoral Program, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Natarajan, Bharath] NIST, Ctr Nanoscale Sci & Technol, Gaithersburg, MD 20899 USA.
[McCorkle, Linda S.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
RP Williams, TS (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Cleveland, OH 44135 USA.
EM tiffany.s.williams@nasa.gov
RI Liddle, James/A-4867-2013;
OI Liddle, James/0000-0002-2508-7910; Obrzut, Jan/0000-0001-6667-9712
FU NASA Game Changing Development Program/Nanotechnology Project; NASA
Postdoctoral Program at the NASA Glenn Research Center - Oak Ridge
Associated Universities; Rice University [70NANB12H188]; National
Institute of Standards and Technology [70NANB12H188]
FX This effort was funded through the NASA Game Changing Development
Program/Nanotechnology Project. Support was also received from the
following sources: the NASA Postdoctoral Program at the NASA Glenn
Research Center sponsored by Oak Ridge Associated Universities, and a
Cooperative Research Agreement between Rice University and the National
Institute of Standards and Technology (grant 70NANB12H188). We thank Dr.
Jeffrey Eldrige for assistance with Raman Spectroscopy and Nathan
Wilmoth for his assistance with mechanical testing. Microwave
spectroscopy measurements were carried out at the NIST Materials
Measurement Laboratory in support of the National Nano technology
Initiative.
NR 35
TC 0
Z9 0
U1 4
U2 8
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1944-8244
J9 ACS APPL MATER INTER
JI ACS Appl. Mater. Interfaces
PD APR 13
PY 2016
VL 8
IS 14
BP 9327
EP 9334
DI 10.1021/acsami.5b12303
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA DJ5UF
UT WOS:000374274900057
PM 27044063
ER
PT J
AU Huang, NE
Hu, K
Yang, ACC
Chang, HC
Jia, D
Liang, WK
Yeh, JR
Kao, CL
Juan, CH
Peng, CK
Meijer, JH
Wang, YH
Long, SR
Wu, ZH
AF Huang, Norden E.
Hu, Kun
Yang, Albert C. C.
Chang, Hsing-Chih
Jia, Deng
Liang, Wei-Kuang
Yeh, Jia Rong
Kao, Chu-Lan
Juan, Chi-Hung
Peng, Chung Kang
Meijer, Johanna H.
Wang, Yung-Hung
Long, Steven R.
Wu, Zhauhua
TI On Holo-Hilbert spectral analysis: a full informational spectral
representation for nonlinear and non-stationary data
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Article
DE Hilbert-Huang transform; nonlinear; non-stationary; empirical mode
decomposition; Holo-Hilbert spectrum; Holo-Hilbert spectral analysis
ID EMPIRICAL MODE DECOMPOSITION; TIME-SERIES
AB The Holo-Hilbert spectral analysis (HHSA) method is introduced to cure the deficiencies of traditional spectral analysis and to give a full informational representation of nonlinear and non-stationary data. It uses a nested empirical mode decomposition and Hilbert-Huang transform (HHT) approach to identify intrinsic amplitude and frequency modulations often present in nonlinear systems. Comparisons are first made with traditional spectrum analysis, which usually achieved its results through convolutional integral transforms based on additive expansions of an a priori determined basis, mostly under linear and stationary assumptions. Thus, for non-stationary processes, the best one could do historically was to use the time-frequency representations, in which the amplitude (or energy density) variation is still represented in terms of time. For nonlinear processes, the data can have both amplitude and frequency modulations (intra-mode and inter-mode) generated by two different mechanisms: linear additive or nonlinear multiplicative processes. As all existing spectral analysis methods are based on additive expansions, either a priori or adaptive, none of them could possibly represent the multiplicative processes. While the earlier adaptive HHT spectral analysis approach could accommodate the intra-wave nonlinearity quite remarkably, it remained that any inter-wave nonlinear multiplicative mechanisms that include cross-scale coupling and phase-lock modulations were left untreated. To resolve the multiplicative processes issue, additional dimensions in the spectrum result are needed to account for the variations in both the amplitude and frequency modulations simultaneously. HHSA accommodates all the processes: additive and multiplicative, intra-mode and inter-mode, stationary and non-stationary, linear and nonlinear interactions. The Holo prefix in HHSA denotes a multiple dimensional representation with both additive and multiplicative capabilities.
C1 [Huang, Norden E.; Chang, Hsing-Chih; Yeh, Jia Rong; Kao, Chu-Lan; Wang, Yung-Hung] Natl Cent Univ, Res Ctr Adapt Data Anal, Zhongli 32001, Taiwan.
[Liang, Wei-Kuang; Juan, Chi-Hung] Natl Cent Univ, Grad Inst Cognit Neurosci, Zhongli 32001, Taiwan.
[Hu, Kun] Univ Hartford, Brigham & Womens Hosp, Div Sleep Med, Med Biodynam Program,Med Sch, 221 Longwood Ave, Boston, MA 02115 USA.
[Yang, Albert C. C.] Taipei Vet Gen Hosp, Dept Psychiat, Shipai 11217, Taiwan.
[Jia, Deng] SOA, Res Inst Oceanog 1, Qingdao 266061, Peoples R China.
[Peng, Chung Kang] Harvard Univ, Beth Israel Deaconess Med Ctr, Sch Med, 330 Brookline Ave, Boston, MA 02215 USA.
[Meijer, Johanna H.] Leiden Univ, Med Ctr, Neurophysiol Lab, Dept Mol Cell Biol, NL-2300 RC Leiden, Netherlands.
[Long, Steven R.] NASA GSFC, Sci & Explorat Directorate, Field Support Off, Wallops Flight Facil, Code 610-W, Wallops Isl, VA 23337 USA.
[Wu, Zhauhua] Florida State Univ, Dept Meteorol, 2035 E Paul Dirac Dr,200 RM Johnson Bldg, Tallahassee, FL 32306 USA.
RP Huang, NE (reprint author), Natl Cent Univ, Res Ctr Adapt Data Anal, Zhongli 32001, Taiwan.
EM norden@cc.ncu.edu.tw
OI Wu, Zhaohua/0000-0003-1660-0724
FU National Science Council, Taiwan [NSC 101-2911-I-008-100]; NCU, under
the programme of Center of Excellence from MoE
FX This study has been supported by a grant for the Center for Dynamical
Biomarkers and Translational Medicine, National Central University,
Taiwan (NSC 101-2911-I-008-100) from the National Science Council,
Taiwan, and a grant from NCU, under the programme of Center of
Excellence from MoE, which have made the conclusion of this study
possible.
NR 16
TC 5
Z9 6
U1 7
U2 25
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-503X
EI 1471-2962
J9 PHILOS T R SOC A
JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci.
PD APR 13
PY 2016
VL 374
IS 2065
AR 20150206
DI 10.1098/rsta.2015.0206
PG 21
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DH1OC
UT WOS:000372553500012
PM 26953180
ER
PT J
AU Michal, BT
Brenn, WA
Nguyen, BN
McCorkle, LS
Meador, MAB
Rowan, SJ
AF Michal, Brian T.
Brenn, William A.
Nguyen, Baochau N.
McCorkle, Linda S.
Meador, Mary Ann B.
Rowan, Stuart J.
TI Thermoresponsive Shape-Memory Aerogels from Thiol-Ene Networks
SO CHEMISTRY OF MATERIALS
LA English
DT Article
ID POLYIMIDE AEROGELS; MECHANICALLY STRONG; POLYMER; POLYMERIZATIONS;
SCAFFOLD; FOAM
AB Thermoresponsive shape-memory polymer aerogels have been produced from thiol-ene networks of 1,6-hexanedithiol, pentaerythritol tetrakis(3-mercaptopropionate), and triallyl-1,3,5-triazine-2,4,6-trione. The thiol-ene networks form organogels with either acetonitrile or acetone as the solvent, which can be subsequently removed using supercritical CO2 extraction. The resulting aerogels have nearly quantitative shape fixing and shape recovery with a glass transition temperature ranging from 42 to 64 degrees C, which serves as the thermal transition trigger for the shape-memory effect. The aerogels have a porosity of 72% to 81% but surface areas of only 5-10 m(2)/g.
C1 [Michal, Brian T.; Brenn, William A.; Rowan, Stuart J.] Case Western Reserve Univ, Dept Macromol Sci & Engn, 2100 Adelbert Rd, Cleveland, OH 44106 USA.
[Meador, Mary Ann B.] NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
[Nguyen, Baochau N.; McCorkle, Linda S.] Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.
RP Rowan, SJ (reprint author), Case Western Reserve Univ, Dept Macromol Sci & Engn, 2100 Adelbert Rd, Cleveland, OH 44106 USA.
EM stuart.rowan@case.edu
OI Meador, Mary Ann/0000-0003-2513-7372
FU National Aeronautics and Space Administration [NNX11AN5OH]; Kent H.
Smith Charitable Trust
FX The authors gratefully acknowledge financial support from the National
Aeronautics and Space Administration (Grant No. NNX11AN5OH to BTM) and
the Kent H. Smith Charitable Trust.
NR 44
TC 0
Z9 0
U1 32
U2 63
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0897-4756
EI 1520-5002
J9 CHEM MATER
JI Chem. Mat.
PD APR 12
PY 2016
VL 28
IS 7
BP 2341
EP 2347
DI 10.1021/acs.chemmater.6b00474
PG 7
WC Chemistry, Physical; Materials Science, Multidisciplinary
SC Chemistry; Materials Science
GA DJ4RS
UT WOS:000374196000048
ER
PT J
AU Alpaslan, M
Grootes, M
Marcum, PM
Popescu, C
Tuffs, R
Bland-Hawthorn, J
Brough, S
Brown, MJI
Davies, LJM
Driver, SP
Holwerda, BW
Kelvin, LS
Lara-Lopez, MA
Lopez-Sanchez, AR
Loveday, J
Moffett, A
Taylor, EN
Owers, M
Robotham, ASG
AF Alpaslan, Mehmet
Grootes, Meiert
Marcum, Pamela M.
Popescu, Cristina
Tuffs, Richard
Bland-Hawthorn, Joss
Brough, Sarah
Brown, Michael J. I.
Davies, Luke J. M.
Driver, Simon P.
Holwerda, Benne W.
Kelvin, Lee S.
Lara-Lopez, Maritza A.
Lopez-Sanchez, Angel R.
Loveday, Jon
Moffett, Amanda
Taylor, Edward N.
Owers, Matt
Robotham, Aaron S. G.
TI Galaxy And Mass Assembly (GAMA): stellar mass growth of spiral galaxies
in the cosmic web
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: spiral; galaxies: stellar content; large-scale structure of
Universe
ID LARGE-SCALE STRUCTURE; DIGITAL SKY SURVEY; HALO OCCUPATION DISTRIBUTION;
STAR-FORMATION ACTIVITY; LOCAL UNIVERSE; VOID GALAXIES; DATA RELEASE;
DARK-MATTER; LUMINOSITY FUNCTION; FILAMENTS
AB We look for correlated changes in stellar mass and star formation rate (SFR) along filaments in the cosmic web by examining the stellar masses and UV-derived SFRs of 1799 ungrouped and unpaired spiral galaxies that reside in filaments. We devise multiple distance metrics to characterize the complex geometry of filaments, and find that galaxies closer to the cylindrical centre of a filament have higher stellar masses than their counterparts near the periphery of filaments, on the edges of voids. In addition, these peripheral spiral galaxies have higher SFRs at a given mass. Complementing our sample of filament spiral galaxies with spiral galaxies in tendrils and voids, we find that the average SFR of these objects in different large-scale environments are similar to each other with the primary discriminant in SFR being stellar mass, in line with previous works. However, the distributions of SFRs are found to vary with large-scale environment. Our results thus suggest a model in which in addition to stellar mass as the primary discriminant, the large-scale environment is imprinted in the SFR as a second-order effect. Furthermore, our detailed results for filament galaxies suggest a model in which gas accretion from voids on to filaments is primarily in an orthogonal direction. Overall, we find our results to be in line with theoretical expectations of the thermodynamic properties of the intergalactic medium in different large-scale environments.
C1 [Alpaslan, Mehmet; Marcum, Pamela M.] NASA, Ames Res Ctr, Moffett Field, N232, Mountain View, CA 94035 USA.
[Grootes, Meiert; Popescu, Cristina; Tuffs, Richard] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany.
[Popescu, Cristina] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Popescu, Cristina] Astron Inst Romanian Acad, Str Cutitul Argint 5, Bucharest 040557, Romania.
[Bland-Hawthorn, Joss] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Brough, Sarah; Lopez-Sanchez, Angel R.; Owers, Matt] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia.
[Brown, Michael J. I.] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia.
[Davies, Luke J. M.; Driver, Simon P.; Moffett, Amanda; Robotham, Aaron S. G.] Univ Western Australia, Int Ctr Radio Astron Res, 7 Fairway, Perth, WA 6009, Australia.
[Holwerda, Benne W.] Leiden Univ, Sterrenwacht Leiden, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
[Kelvin, Lee S.] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England.
[Lara-Lopez, Maritza A.] Univ Nacl Autonoma Mexico, Inst Astron, AP 70-264, Mexico City 04150, DF, Mexico.
[Lopez-Sanchez, Angel R.; Owers, Matt] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia.
[Loveday, Jon] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Taylor, Edward N.] Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia.
RP Alpaslan, M (reprint author), NASA, Ames Res Ctr, Moffett Field, N232, Mountain View, CA 94035 USA.
EM mehmet.alpaslan@nasa.gov
RI Brown, Michael/B-1181-2015
OI Brown, Michael/0000-0002-1207-9137
FU UNAM through the PAPIIT [IA101315]; STFC (UK); ARC (Australia); AAO;
NASA; ESO Telescopes at the La Silla Paranal Observatory [179.A-2004]
FX MA is funded by an appointment to the NASA Postdoctoral Program at Ames
Research Centre, administered by Oak Ridge Associated Universities
through a contract with NASA. MALL acknowledges support from UNAM
through the PAPIIT project IA101315. The authors would like to thank the
anonymous referee, whose contributions have helped to improve this
work.; GAMA is a joint European-Australasian project based around a
spectroscopic campaign using the Anglo-Australian Telescope. The GAMA
input catalogue is based on data taken from the Sloan Digital Sky Survey
and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the
GAMA regions is being obtained by a number of independent survey
programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE,
Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is
funded by the STFC (UK), the ARC (Australia), the AAO and the
participating institutions. The GAMAwebsite is
http://www.gama-survey.org/. The VISTA VIKING data used in this paper
are based on observations made with ESO Telescopes at the La Silla
Paranal Observatory under programme ID 179.A-2004.
NR 83
TC 3
Z9 3
U1 2
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 11
PY 2016
VL 457
IS 3
BP 2287
EP 2300
DI 10.1093/mnras/stw134
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6BJ
UT WOS:000373583900002
ER
PT J
AU Clampitt, J
Miyatake, H
Jain, B
Takada, M
AF Clampitt, Joseph
Miyatake, Hironao
Jain, Bhuvnesh
Takada, Masahiro
TI Detection of stacked filament lensing between SDSS luminous red galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; cosmology: observations; dark matter;
large-scale structure of Universe
ID COSMIC WEB; DARK-MATTER; ELLIPTICITY; STATISTICS; HALOS; PAIRS
AB We search for the lensing signal of massive filaments between 135 000 pairs of luminous red galaxies (LRGs) from the Sloan Digital Sky Survey. We develop a new estimator that cleanly removes the much larger shear signal of the neighbouring LRG haloes, relying only on the assumption of spherical symmetry. We consider two models: a 'thick'-filament model constructed from ray-tracing simulations for A cold dark matter model, and a 'thin'-filament model which models the filament by a string of haloes along the line connecting the two LRGs. We show that the filament lensing signal is in nice agreement with the thick simulation filament, while strongly disfavouring the thin model. The magnitude of the lensing shear due to the filament is below 10(-4). Employing the likelihood ratio test, we find a 4.5 sigma significance for the detection of the filament lensing signal, corresponding to a null hypothesis fluctuation probability of 3 x 10(-6). We also carried out several null tests to verify that the residual shear signal from neighbouring LRGs and other shear systematics are minimized.
C1 [Clampitt, Joseph; Jain, Bhuvnesh] Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA.
[Miyatake, Hironao] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Miyatake, Hironao; Takada, Masahiro] Univ Tokyo, Univ Kavli IPMU WPI, Kavli Inst Phys & Math, Chiba 2778583, Japan.
[Miyatake, Hironao] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Clampitt, J (reprint author), Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA.
EM clampitt@sas.upenn.edu
FU NSF [1066293]; Department of Energy [DE-SC0007901]; World Premier
International Research Center Initiative (WPI Initiative), MEXT, Japan;
FIRST program 'Subaru Measurements of Images and Redshifts (SuMIRe)',
CSTP, Japan; JSPS Promotion of Science [23340061, 26610058]; MEXT
[15H05893, 15K21733]; Japan Society for the Promotion of Science (JSPS);
Jet Propulsion Laboratory, California Institute of Technology; National
Aeronautics and Space Administration
FX We would like to thank Gary Bernstein, Sarah Bridle, Jorg Dietrich, Mike
Jarvis, Elisabeth Krause, Ravi Sheth, Yuanyuan Zhang, and especially
Rachel Mandelbaum for helpful discussions and comments. We are very
grateful to Erin Sheldon for the use of his SDSS shear catalogues and to
Tomasz Kacprzak for related collaborative work. BJ and MT also thank the
Aspen Center for Physics and NSF Grant #1066293, for their warm
hospitality when part of this work was done. BJ and JC are partially
supported by Department of Energy grant DE-SC0007901. MT is supported by
World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan, by the FIRST program 'Subaru Measurements of Images and
Redshifts (SuMIRe)', CSTP, Japan, by Grant-in-Aid for Scientific
Research from the JSPS Promotion of Science (No. 23340061 and 26610058),
and by MEXT Grant-in-Aid for Scientific Research on Innovative Areas
(No. 15H05893 and 15K21733). HM was supported in part by Japan Society
for the Promotion of Science (JSPS) Research Fellowships for Young
Scientists. HM was supported in part by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 23
TC 3
Z9 3
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 11
PY 2016
VL 457
IS 3
BP 2391
EP 2400
DI 10.1093/mnras/stw142
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6BJ
UT WOS:000373583900009
ER
PT J
AU Boldrin, M
Giocoli, C
Meneghetti, M
Moscardini, L
Tormen, G
Biviano, A
AF Boldrin, Michele
Giocoli, Carlo
Meneghetti, Massimo
Moscardini, Lauro
Tormen, Giuseppe
Biviano, Andrea
TI Cosmology through arc statistics I: sensitivity to Omega(m) and sigma(8)
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: strong; galaxies: clusters: general; cosmology:
theory
ID DARK-MATTER HALOES; CONCENTRATION-MASS RELATION; LENSING CROSS-SECTIONS;
DIGITAL SKY SURVEY; GALAXY CLUSTERS; CONSTRAINTS; SIMULATIONS; SAMPLE;
UNIVERSALITY; POPULATION
AB The next generation of large sky photometric surveys will finally be able to use arc statistics as a cosmological probe. Here, we present the first of a series of papers on this topic. In particular, we study how arc counts are sensitive to the variation of two cosmological parameters: the (total) matter density parameter, Omega(m), and the normalization of the primordial power spectrum, expressed in terms of as. Both these parameters influence the abundances of collapsed structures and their internal structure. We compute the expected number of gravitational arcs with various length-to-width ratios in mock light cones, by varying these cosmological parameters in the ranges 0.1 <= Omega(m) < 0.5 and 0.6 <= sigma(8) <= 1. We find that the arc counts dependence on Omega(m) and as is similar, but not identical, to that of the halo counts. We investigate how the precision of the constraints on the cosmological parameters based on arc counts depend on the survey area. We find that the constraining power of arc statistics degrades critically only for surveys covering an area smaller than 10 per cent of the whole sky. Finally, we consider the case in which the search for arcs is done only in frames where galaxy clusters have been previously identified. Adopting the selection function for galaxy clusters expected to be detected from photometric data in future wide surveys, we find that less than 10 per cent of the arcs will be missed, with only a small degradation of the corresponding cosmological constraints.
C1 [Boldrin, Michele; Tormen, Giuseppe] Univ Padua, Dipartimento Fis & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy.
[Giocoli, Carlo; Moscardini, Lauro] Alma Mater Studiorum Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Giocoli, Carlo; Moscardini, Lauro] INFN Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Giocoli, Carlo; Meneghetti, Massimo; Moscardini, Lauro] INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy.
[Giocoli, Carlo] Aix Marseille Univ, LAM, CNRS, UMR 7326, F-13388 Marseille, France.
[Meneghetti, Massimo] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Biviano, Andrea] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy.
RP Boldrin, M (reprint author), Univ Padua, Dipartimento Fis & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy.
EM michele.boldrin@studenti.unipd.it
FU European Seventh Framework Programme [259349]; CNES; PRIN MIUR; PRIN
INAF [2014 1.05.01.94.02]; [ASI/INAF/I/023/12/0]
FX We thank Barbara Sartoris, Cosimo Fedeli and Peter Schneider for useful
discussions on the Euclid cluster selection function. CG's research is
part of the project GLENCO, funded under the European Seventh Framework
Programme, Ideas, Grant Agreement no. 259349. CG thanks CNES for
financial support. MM and LM acknowledge financial contributions from
contracts ASI/INAF/I/023/12/0, by the PRIN MIUR 2010-2011 'The dark
Universe and the cosmic evolution of baryons: from current surveys to
Euclid' and by the PRIN INAF 2012. We acknowledge support from PRIN-INAF
2014 1.05.01.94.02. We are grateful to the referee Prasenjit Saha for
his useful comments.
NR 58
TC 1
Z9 1
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 11
PY 2016
VL 457
IS 3
BP 2738
EP 2748
DI 10.1093/mnras/stw140
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6BJ
UT WOS:000373583900033
ER
PT J
AU Srinivasan, S
Boyer, ML
Kemper, F
Meixner, M
Sargent, BA
Riebel, D
AF Srinivasan, S.
Boyer, M. L.
Kemper, F.
Meixner, M.
Sargent, B. A.
Riebel, D.
TI The evolved-star dust budget of the Small Magellanic Cloud: the critical
role of a few key players
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: AGB and post-AGB-stars: carbon; stars: mass-loss; supergiants;
Magellanic Clouds
ID ASYMPTOTIC GIANT BRANCH; MASS-LOSS RETURN; NEAR-INFRARED PHOTOMETRY;
YOUNG STELLAR OBJECTS; GALAXY EVOLUTION; AGB STARS; LOW METALLICITY;
CARBON STARS; MU-M; OPTICAL SPECTROSCOPY
AB The life cycle of dust in the interstellar medium is heavily influenced by outflows from asymptotic giant branch (AGB) and red supergiant (RSG) stars, a large fraction of which is contributed by a few very dusty sources. We compute the dust input to the Small Magellanic Cloud (SMC) by fitting the multi-epoch mid-infrared spectral energy distributions of AGB/RSG candidates with models from the Grid of RSG and AGB ModelS grid, allowing us to estimate the luminosities and dust-production rates (DPRs) of the entire population. By removing contaminants, we guarantee a high-quality data set with reliable DPRs and a complete inventory of the dustiest sources. We find a global AGB/RSG dust-injection rate of (1.3 +/- 0.1) x 10(-6) M-circle dot yr(-1), in agreement with estimates derived from mid -infrared colours and excess fluxes. As in the Large Magellanic Cloud, a majority (66 per cent) of the dust arises from the extreme AGB stars, which comprise only per cent of our sample. A handful of far -infrared sources, whose 24 mu m fluxes exceed their 8 m fluxes, dominate the dust input. Their inclusion boosts the global DPR by approximate to 1.5x, making it necessary to determine whether they are AGB stars. Model assumptions, rather than missing data, are the major sources of uncertainty; depending on the choice of dust shell expansion speed and dust optical constants, the global DPR can be up to approximate to 10 times higher. Our results suggest a non-stellar origin for the SMC dust, barring as yet undiscovered evolved stars with very high DPRs.
C1 [Srinivasan, S.; Kemper, F.] Acad Sinica, Inst Astron & Astrophys, 11F,Astron Math Bldg 1,Roosevelt Rd,Sec 4, Taipei 10617, Taiwan.
[Boyer, M. L.] NASA, Goddard Space Flight Ctr, CRESST, Code 665, Greenbelt, MD 20771 USA.
[Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
[Boyer, M. L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Meixner, M.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Sargent, B. A.] Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA.
[Sargent, B. A.] Rochester Inst Technol, Lab Multiwavelength Astrophys, 54 Lomb Mem Dr, Rochester, NY 14623 USA.
[Riebel, D.] US Naval Acad, Dept Phys, 572C Holloway Rd, Annapolis, MD 21402 USA.
RP Srinivasan, S (reprint author), Acad Sinica, Inst Astron & Astrophys, 11F,Astron Math Bldg 1,Roosevelt Rd,Sec 4, Taipei 10617, Taiwan.
EM sundar@asiaa.sinica.edu.tw
RI Kemper, Francisca/D-8688-2011
OI Kemper, Francisca/0000-0003-2743-8240
FU SAGE-LMC Spitzer grant [1275598]; NASA Postdoctoral Program at the
Goddard Space Flight Center; NASA; Ministry of Science and Technology in
Taiwan [MOST103-2112-M-001-033-, MOST104-2628-M-001-004-MY3]; NASA ADAP
grant [NNX13AE36G, NNX13AD54G]; NASA [1407]; National Aeronautics and
Space Administration; NSF; NASA's Astrophysics Data System Bibliographic
Services; [NAG5-12595]
FX We are grateful to the anonymous referee for their thorough and helpful
comments. We thank Lynn Carlson for her insight on separating YSOs from
AGB candidates in colour-magnitude and colour-colour diagrams. We
acknowledge funding from the NAG5-12595 grant and the SAGE-LMC Spitzer
grant 1275598. MLB is supported by the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by ORAU through a contract
with NASA. FK acknowledges financial support by the Ministry of Science
and Technology in Taiwan, under grant codes MOST103-2112-M-001-033- and
MOST104-2628-M-001-004-MY3. MM acknowledges the NASA ADAP grant
NNX13AE36G. BAS acknowledges the NASA ADAP grant NNX13AD54G. The authors
would also like to thank Bernie Shiao at STScI for his invaluable
assistance with the SAGE database. This work is based on observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under NASA
contract 1407. The publication makes use of data products from the Wide
field Infrared Survey Explorer, which is a joint project of the
University of California, Los Angeles, and the Jet Propulsion
Laboratory/California Institute of Technology, funded by the National
Aeronautics and Space Administration. This research has also made use of
the SAGE CASJobs database, which is made possible by the Sloan Digital
Sky Survey Collaboration; SAOImage DS9, developed by the Smithsonian
Astrophysical Observatory; the Vizier catalogue access tool, CDS,
Strasbourg, France; the SIMBAD database, operated at CDS, Strasbourg,
France; the cross-match tool available through the US Virtual
Astronomical Observatory, which is sponsored by the NSF and NASA; and
NASA's Astrophysics Data System Bibliographic Services.
NR 76
TC 3
Z9 3
U1 2
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 11
PY 2016
VL 457
IS 3
BP 2814
EP 2838
DI 10.1093/mnras/stw155
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6BJ
UT WOS:000373583900038
ER
PT J
AU Evans, A
Gehrz, RD
Woodward, CE
Sarre, PJ
van Loon, JT
Helton, LA
Starrfield, S
Eyres, SPS
AF Evans, A.
Gehrz, R. D.
Woodward, C. E.
Sarre, P. J.
van Loon, J. T.
Helton, L. A.
Starrfield, S.
Eyres, S. P. S.
TI CK Vul: a smorgasbord of hydrocarbons rules out a 1670 nova (and much
else besides)
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE circumstellar matter; stars: individual: CK Vul; ISM: molecules;
infrared: stars
ID SPITZER-SPACE-TELESCOPE; PLANETARY-NEBULAE; CLASSICAL NOVAE; DUST;
EMISSION; EVOLUTION; MOLECULES; FEATURES; STARS; PAHS
AB We present observations of CK Vul obtained with the Spitzer Space Telescope. The infrared spectrum reveals a warm dust continuum with nebular, molecular hydrogen and HCN lines superimposed, together with the 'Unidentified Infrared' features. The nebular lines are consistent with emission by a low-density gas. We conclude that the Spitzer data, combined with other information, are incompatible with CK Vul being a classical nova remnant in 'hibernation' after the event of 1670, a 'very late thermal pulse', a 'Luminous Red Variable', such as V838 Mon, or a 'diffusion-induced nova'. The true nature of CK Vul remains a mystery.
C1 [Evans, A.; van Loon, J. T.] Keele Univ, Lennard Jones Lab, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Gehrz, R. D.; Woodward, C. E.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, 116 Church St SE, Minneapolis, MN 55455 USA.
[Sarre, P. J.] Univ Nottingham, Sch Chem, Univ Pk, Nottingham NG7 2RD, England.
[Helton, L. A.] NASA, Ames Res Ctr, USRA SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Box 871404, Tempe, AZ 85287 USA.
[Eyres, S. P. S.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
RP Evans, A (reprint author), Keele Univ, Lennard Jones Lab, Astrophys Grp, Keele ST5 5BG, Staffs, England.
EM a.evans@keele.ac.uk
FU NASA; United States Air Force; Leverhulme Trust; NSF; Spitzer grants
FX We thank the referee for helpful comments which have helped to improve
the Paper. RDG was supported by NASA and the United States Air Force.
CEW was supported in part by NASA Spitzer grants to the University of
Minnesota. PJS thanks the Leverhulme Trust for award of a Research
Fellowship. SS acknowledges partial support from NASA, NSF and Spitzer
grants to ASU.
NR 51
TC 0
Z9 0
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 11
PY 2016
VL 457
IS 3
BP 2871
EP 2876
DI 10.1093/mnras/stw352
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6BJ
UT WOS:000373583900043
ER
PT J
AU Harding, LK
Hallinan, G
Milburn, J
Gardner, P
Konidaris, N
Singh, N
Shao, M
Sandhu, J
Kyne, G
Schlichting, HE
AF Harding, L. K.
Hallinan, G.
Milburn, J.
Gardner, P.
Konidaris, N.
Singh, N.
Shao, M.
Sandhu, J.
Kyne, G.
Schlichting, H. E.
TI CHIMERA: a wide-field, multi-colour, high-speed photometer at the prime
focus of the Hale telescope
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE instrumentation: detectors; instrumentation: photometers; methods:
observational; techniques: photometric; occultations
ID STELLAR SCINTILLATION; SYSTEM; CAMERA; EMISSION
AB The Caltech HIgh-speed Multi-colour camERA (CHIMERA) is a newinstrument that has been developed for use at the prime focus of the Hale 200-inch telescope. Simultaneous optical imaging in two bands is enabled by a dichroic beam splitter centred at 567 nm, with Sloan u' and g' bands available on the blue arm and Sloan r', i' and z_s bands available on the red arm. Additional narrow-band filters will also become available as required. An electron multiplying CCD (EMCCD) detector is employed for both optical channels, each capable of simultaneously delivering sub-electron effective read noise under multiplication gain and frame rates of up to 26 fps full frame (several 1000 fps windowed), over a fully corrected 5 x 5 arcmin field of view. CHIMERA was primarily developed to enable the characterization of the size distribution of sub-km Kuiper Belt Objects via stellar occultation, a science case that motivates the frame-rate, the simultaneous multi-colour imaging and the wide field of view of the instrument. In addition, it also has unique capability in the detection of faint near-Earth asteroids and will be used for the monitoring of short-duration transient and periodic sources, particularly those discovered by the intermediate Palomar Transient Factory (iPTF), and the upcoming Zwicky Transient Facility (ZTF).
C1 [Harding, L. K.; Hallinan, G.; Milburn, J.; Gardner, P.; Konidaris, N.; Singh, N.; Kyne, G.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Harding, L. K.; Singh, N.; Shao, M.; Sandhu, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schlichting, H. E.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
RP Harding, LK; Hallinan, G (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.; Harding, LK (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM leon.k.harding@jpl.nasa.gov; gh@astro.caltech.edu
FU JPL RTD; National Aeronautics and Space Administration
FX The authors gratefully acknowledge the support of the Caltech Optical
Observatories. We would especially like to thank Richard Dekaney and
Christoph Baranec, for their extremely helpful advice throughout the
CHIMERA project. We would like to highlight the excellent support of the
Palomar Observatory staff, particularly John Henning, Steve Kunsman,
Mike Doyle, Kevin Rykoski, Bruce Baker, Jamey Eriksen, Carolyn Heffner,
Dan McKenna, Jean Mueller, Kajsa Peffer and Greg Van Idsinga. We also
acknowledge Steve Macenka and James McGuire for their helpful
contribution. The work described here was carried out at the California
Institute of Technology and the Jet Propulsion Laboratory, California
Institute of Technology, under a JPL R&TD grant and a contract with the
National Aeronautics and Space Administration.
NR 35
TC 1
Z9 1
U1 2
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 11
PY 2016
VL 457
IS 3
BP 3036
EP 3049
DI 10.1093/mnras/stw094
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6BJ
UT WOS:000373583900057
ER
PT J
AU Deacon, NR
Schlieder, JE
Murphy, SJ
AF Deacon, N. R.
Schlieder, J. E.
Murphy, S. J.
TI A nearby young M dwarf with a wide, possibly planetary-mass companion
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE planets and satellites: detection; binaries: visual; brown dwarfs;
stars: pre-main-sequence
ID INFRARED-SURVEY-EXPLORER; VERY-LOW-MASS; SUBSTELLAR CANDIDATE MEMBERS;
PRE-MAIN-SEQUENCE; BROWN DWARF; KINEMATIC GROUPS; MOVING GROUPS;
ULTRACOOL DWARFS; STAR CANDIDATES; BETA-PICTORIS
AB We present the identification of two previously known young objects in the solar neighbourhood as a likely very wide binary. TYC 9486-927-1, an active, rapidly rotating early-M dwarf, and 2MASS J21265040-8140293, a low-gravity L3 dwarf previously identified as candidate members of the similar to 45 Myr old Tucana-Horologium association (TucHor). An updated proper motion measurement of the L3 secondary, and a detailed analysis of the pair's kinematics in the context of known nearby, young stars, reveals that they share common proper motion and are likely bound. New observations and analyses reveal the primary exhibits Li 6708 angstrom absorption consistent with M dwarfs younger than TucHor but older than the similar to 10 Myr TW Hydra association yielding an age range of 10-45 Myr. A revised kinematic analysis suggests the space motions and positions of the pair are closer to, but not entirely in agreement with, the similar to 24 Myr old beta Pictoris moving group. This revised 10-45 Myr age range yields a mass range of 11.6-15 M-I for the secondary. It is thus likely 2MASS J2126-8140 is the widest orbit planetary-mass object known (>4500 au) and its estimated mass, age, spectral type, and T-eff are similar to the well-studied planet beta Pictoris b. Because of their extreme separation and youth, this low-mass pair provide an interesting case study for very wide binary formation and evolution.
C1 [Deacon, N. R.] Univ Hertfordshire, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England.
[Schlieder, J. E.] NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA.
[Schlieder, J. E.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Murphy, S. J.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
RP Deacon, NR (reprint author), Univ Hertfordshire, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England.
EM n.deacon2@herts.ac.uk
FU National Aeronautics and Space Administration; National Science
Foundation; Planetary Science Division of the National Aeronautics and
Space Administration; European Commission [CT920791, CT940627]; INSU in
France; MEN in France; CNRS in France; State of Baden-Wurttemberg in
Germany; DGICYT in Spain; CNR in Italy; FFwFBWF in Austria; FAPESP in
Brazil; OTKA in Hungary [F-4239, F-013990]; ESO CEE [A-04-046]; NASA;
[090.A-9010]
FX This research made use of the SIMBAD data base, operated at CDS,
Strasbourg, France. This publication makes use of data products from the
2MASS, which is a joint project of the University of Massachusetts and
the Infrared Processing and Analysis Center/California Institute of
Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation. This publication also makes use of
data products from NEOWISE, which is a project of the Jet Propulsion
Laboratory/California Institute of Technology, funded by the Planetary
Science Division of the National Aeronautics and Space Administration.
The DENIS project has been partly funded by the SCIENCE and the HCM
plans of the European Commission under grants CT920791 and CT940627. It
is supported by INSU, MEN, and CNRS in France, by the State of
Baden-Wurttemberg in Germany, by DGICYT in Spain, by CNR in Italy, by
FFwFBWF in Austria, by FAPESP in Brazil, by OTKA grants F-4239 and
F-013990 in Hungary, and by the ESO C&EE grant A-04-046. Jean Claude
Renault from IAP was the Project manager. Observations were carried out
thanks to the contribution of numerous students and young scientists
from all involved institutes, under the supervision of P. Fouque, survey
astronomer resident in Chile. Based on observations obtained at the
Gemini Observatory (PID GS-2009B-C-2, acquired through the Gemini
Science Archive), which is operated by the Association of Universities
for Research in Astronomy, Inc., under a cooperative agreement with the
NSF on behalf of the Gemini partnership: the National Science Foundation
(United States), the National Research Council (Canada), CONICYT
(Chile), the Australian Research Council (Australia), Ministerio da
Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia,
Tecnologia e Innovacion Productiva (Argentina). The research of JES was
supported by an appointment to the NASA Postdoctoral Program at NASA
Ames Research Center, administered by Oak Ridge Associated Universities
through a contract with NASA. We thank the anonymous referee for the
prompt and helpful review that improved the quality and clarity of this
manuscript. The authors would like to thank the Brass Monkey, Heidelberg
for the opportunity to pit their wits against each other every week.
Based on observations made with the ESO/MPG 2.2 m telescope at the La
Silla Observatory under programme ID 090.A-9010.
NR 54
TC 6
Z9 6
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 11
PY 2016
VL 457
IS 3
BP 3191
EP 3199
DI 10.1093/mnras/stw172
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6BJ
UT WOS:000373583900070
ER
PT J
AU Schaan, E
Ferraro, S
Vargas-Magana, M
Smith, KM
Ho, S
Aiola, S
Battaglia, N
Bond, JR
De Bernardis, F
Calabrese, E
Cho, HM
Devlin, MJ
Dunkley, J
Gallardo, PA
Hasselfield, M
Henderson, S
Hill, JC
Hincks, AD
Hlozek, R
Hubmayr, J
Hughes, JP
Irwin, KD
Koopman, B
Kosowsky, A
Li, D
Louis, T
Lungu, M
Madhavacheri, M
Maurin, L
McMahon, JJ
Moodley, K
Naess, S
Nati, F
Newburgh, L
Niemack, MD
Page, LA
Pappas, CG
Partridge, B
Schmitt, BL
Sehga, N
Sherwin, BD
Sievers, JL
Spergel, DN
Staggs, ST
van Engelen, A
Wollack, EJ
AF Schaan, Emmanuel
Ferraro, Simone
Vargas-Magana, Mariana
Smith, Kendrick M.
Ho, Shirley
Aiola, Simone
Battaglia, Nicholas
Bond, J. Richard
De Bernardis, Francesco
Calabrese, Erminia
Cho, Hsiao-Mei
Devlin, Mark J.
Dunkley, Joanna
Gallardo, Patricio A.
Hasselfield, Matthew
Henderson, Shawn
Hill, J. Colin
Hincks, Adam D.
Hlozek, Renee
Hubmayr, Johannes
Hughes, John P.
Irwin, Kent D.
Koopman, Brian
Kosowsky, Arthur
Li, Dale
Louis, Thibaut
Lungu, Marius
Madhavacheri, Mathew
Maurin, Loic
McMahon, Jeffrey John
Moodley, Kavilan
Naess, Sigurd
Nati, Federico
Newburgh, Laura
Niemack, Michael D.
Page, Lyman A.
Pappas, Christine G.
Partridge, Bruce
Schmitt, Benjamin L.
Sehga, Neelima
Sherwin, Blake D.
Sievers, Jonathan L.
Spergel, David N.
Staggs, Suzanne T.
van Engelen, Alexander
Wollack, Edward J.
CA ACTPol Collaboration
TI Evidence for the kinematic Sunyaev-Zel'dovich effect with the Atacama
Cosmology Telescope and velocity reconstruction from the Baryon
Oscillation Spectroscopic Survey
SO PHYSICAL REVIEW D
LA English
DT Article
ID LOCALLY BRIGHTEST GALAXIES; WEAK LENSING SIGNAL; DIGITAL SKY SURVEY;
ACOUSTIC-OSCILLATIONS; POWER SPECTRUM; DATA RELEASE; BULK FLOW;
CONSTRAINTS; CLUSTERS; FEEDBACK
AB We use microwave temperature maps from two seasons of data from the Atacama Cosmology Telescope at 146 GHz, together with the "Constant Mass" CMASS galaxy sample from the Baryon Oscillation Spectroscopic Survey to measure the kinematic Sunyaev-Zel'dovich (kSZ) effect over the redshift range z = 0.4-0.7. We use galaxy positions and the continuity equation to obtain a reconstruction of the line-of-sight velocity field. We stack the microwave temperature at the location of each halo, weighted by the corresponding reconstructed velocity. We vary the size of the aperture photometry filter used, thus probing the free electron profile of these halos from within the virial radius out to three virial radii, on the scales relevant for investigating the missing baryons problem. The resulting best fit kSZ model is preferred over the no-kSZ hypothesis at 3.3 and 2.9 sigma for two independent velocity reconstruction methods, using 25,537 galaxies over 660 square degrees. The data suggest that the baryon profile is shallower than the dark matter in the inner regions of the halos probed here, potentially due to energy injection from active galactic nucleus or supernovae. Thus, by constraining the gas profile on a wide range of scales, this technique will be useful for understanding the role of feedback in galaxy groups and clusters. The effect of foregrounds that are uncorrelated with the galaxy velocities is expected to be well below our signal, and residual thermal Sunyaev-Zel'dovich contamination is controlled by masking the most massive clusters. Finally, we discuss the systematics involved in converting our measurement of the kSZ amplitude into the mean free electron fraction of the halos in our sample.
C1 [Schaan, Emmanuel; Ferraro, Simone; Battaglia, Nicholas; Calabrese, Erminia; Hasselfield, Matthew; Hlozek, Renee; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Ferraro, Simone; Sherwin, Blake D.] Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA.
[Vargas-Magana, Mariana] Univ Nacl Autonoma Mexico, Inst Fis, Apartado Postal 20-364, Mexico City 04510, DF, Mexico.
[Smith, Kendrick M.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Ho, Shirley] Carnegie Mellon Univ, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.
[Aiola, Simone; Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Aiola, Simone; Kosowsky, Arthur] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr, Pittsburgh, PA 15260 USA.
[Bond, J. Richard; van Engelen, Alexander] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[De Bernardis, Francesco; Gallardo, Patricio A.; Henderson, Shawn; Koopman, Brian; Maurin, Loic; Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Calabrese, Erminia; Dunkley, Joanna; Louis, Thibaut; Naess, Sigurd] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England.
[Cho, Hsiao-Mei; Irwin, Kent D.; Li, Dale] SLAC Natl Accelerator Lab, 2575 Sandhill Hill Rd, Menlo Pk, CA 94025 USA.
[Devlin, Mark J.; Lungu, Marius; Nati, Federico; Schmitt, Benjamin L.] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA.
[Hill, J. Colin] Columbia Univ, Dept Astron, Pupin Hall, New York, NY 10027 USA.
[Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
[Hubmayr, Johannes] NIST, Boulder, CO 80305 USA.
[Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA.
[Irwin, Kent D.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Madhavacheri, Mathew; Sehga, Neelima] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Maurin, Loic] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile.
[McMahon, Jeffrey John] Univ Michigan, Dept Phys, Ann Arbor, MI 48103 USA.
[Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Newburgh, Laura] Univ Toronto, Dunlap Inst, 50 St George St, Toronto, ON M5S 3H4, Canada.
[Page, Lyman A.; Pappas, Christine G.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Sherwin, Blake D.] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Sherwin, Blake D.] Univ Calif Berkeley, LBL, Dept Phys, Berkeley, CA 94720 USA.
[Sievers, Jonathan L.] Univ KwaZulu Natal, Sch Chem & Phys, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Sievers, Jonathan L.] Univ KwaZulu Natal, NITheP, Private Bag X54001, ZA-4000 Durban, South Africa.
[Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Schaan, E (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
EM eschaan@astro.princeton.edu
RI Wollack, Edward/D-4467-2012; Nati, Federico/I-4469-2016;
OI Wollack, Edward/0000-0002-7567-4451; Nati, Federico/0000-0002-8307-5088;
Aiola, Simone/0000-0002-1035-1854
FU U.S. National Science Foundation (NSF) [AST-0408698, AST-0965625,
PHY-0855887, PHY-1214379]; Princeton University; University of
Pennsylvania; Cornell University; Canada Foundation for Innovation
(CFI); Comision Nacional de Investigacion Cientifica y Tecnologica de
Chile (CONICYT); CFI under the auspices of Compute Canada; Government of
Ontario; Ontario Research Fund Research Excellence; University of
Toronto; Mishrahi Fund; Wilkinson Fund; NSF [AST1311756, AST1517593,
AST1412966, AST-1454881, AST-1517049]; NASA [NNXI2AG72G,
12-EUCLID11-0004, NNX13AE56G, NNX14AB58G, NNX12AM32H, ATP NNX14AB57G];
Government of Canada through Industry Canada; Province of Ontario
through the Ministry of Research and Innovation; NSERC Discovery grant;
DOE-ASC [DOE-DESC001114]; Lyman Spitzer fellowship; ERC [259505]; DOE
[DE-SC0011114]; NASA Space Technology research fellowships; CONICYT
[QUIMAL-120001, FONDECYT-1141113]; Office of Science of the U.S.
Department of Energy [DE-AC02-05CH11231]; Alfred P. Sloan Foundation;
National Science Foundation; U.S. Department of Energy Office of
Science; University of Arizona; Brazilian Participation Group;
Brookhaven National Laboratory; Carnegie Mellon University; University
of Florida; French Participation Group; German Participation Group;
Harvard University; Institute de Astrofisica de Canarias; Michigan
State/Notre Dame/JINA Participation Group; Johns Hopkins University;
Lawrence Berkeley National Laboratory; Max Planck Institute for
Astrophysics; Max Planck Institute for Extraterrestrial Physics; New
Mexico State University; New York University; Ohio State University;
Pennsylvania State University; University of Portsmouth; Spanish
Participation Group; University of Tokyo; University of Utah; Vanderbilt
University; University of Virginia; University of Washington; Yale
University; [AST-1312991]
FX We thank Marcelo Alvarez, Neal Dalal, Tommaso Giannantonio, Oliver Hahn,
Andrey Kravtsov, Guilhem Lavaux, Hironao Miyatake, Hyunbae Park, Hiranya
Peiris, Ue-Li Pen, Bjoern Soergel, Naonori Sugiyama and Simon White for
very useful discussions. This work was supported by the U.S. National
Science Foundation (NSF) through Grants No. AST-0408698 and No.
AST-0965625 for the ACT project, as well as Grants No. PHY-0855887 and
No. PHY-1214379. Funding was also provided by Princeton University, the
University of Pennsylvania, Cornell University and a Canada Foundation
for Innovation (CFI) award to the University of British Columbia.
ACToperates in the Parque Astronomico Atacama in northern Chile under
the auspices of the Comision Nacional de Investigacion Cientifica y
Tecnologica de Chile (CONICYT). Computations were performed on the GPC
supercomputer at the SciNet HPC Consortium. SciNet is funded by the CFI
under the auspices of Compute Canada, the Government of Ontario, the
Ontario Research Fund Research Excellence; and the University of
Toronto. Colleagues at RadioSky provide logistical support and keep
operations in Chile running smoothly. We also thank the Mishrahi Fund
and the Wilkinson Fund for their generous support of the project. E. S.,
S. F. and D. N. S. are supported by NSF Grant No. AST1311756 and NASA
Grant No. NNXI2AG72G. Research at Perimeter Institute is supported by
the Government of Canada through Industry Canada and by the Province of
Ontario through the Ministry of Research and Innovation. K. M. S. was
supported by an NSERC Discovery grant. S. H. is supported in part by
DOE-ASC Award No. DOE-DESC001114, NASA Grant No. 12-EUCLID11-0004, and
NSF Grants No. AST1517593 and No. AST1412966. N. B. acknowledges support
from the Lyman Spitzer fellowship. M. N. and F. D. B. acknowledge
support from NSF Grants No. AST-1454881 and No. AST-1517049. The
development of multichroic detectors and lenses was supported by NASA
Grants No. NNX13AE56G and No. NNX14AB58G. C. M. acknowledges support
from NASA Grant No. NNX12AM32H. Funding from ERC Grant No. 259505
supports S. N., J. D., E. C., and T. L. H. T. is supported by NASA Grant
No. ATP NNX14AB57G, DOE Award No. DE-SC0011114, and NSF Grant No.
AST-1312991. B. S. and B. K. are funded by NASA Space Technology
research fellowships. R. D. received funding from the CONICYT Grants No.
QUIMAL-120001 and No. FONDECYT-1141113. This research used resources of
the National Energy Research Scientific Computing Center, a DOE Office
of Science User Facility supported by the Office of Science of the U.S.
Department of Energy under Award No. DE-AC02-05CH11231. Funding for
SDSS-III has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, and the
U.S. Department of Energy Office of Science. The SDSS-III web site is
http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical
Research Consortium for the Participating Institutions of the SDSS-III
Collaboration including the University of Arizona, the Brazilian
Participation Group, Brookhaven National Laboratory, Carnegie Mellon
University, University of Florida, the French Participation Group, the
German Participation Group, Harvard University, the Institute de
Astrofisica de Canarias, the Michigan State/Notre Dame/JINA
Participation Group, Johns Hopkins University, Lawrence Berkeley
National Laboratory, Max Planck Institute for Astrophysics; Max Planck
Institute for Extraterrestrial Physics, New Mexico State University, New
York University, Ohio State University, Pennsylvania State University,
University of Portsmouth; Princeton University, the Spanish
Participation Group, University of Tokyo, University of Utah, Vanderbilt
University, University of Virginia; University of Washington, and Yale
University.
NR 51
TC 6
Z9 6
U1 4
U2 9
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD APR 11
PY 2016
VL 93
IS 8
AR 082002
DI 10.1103/PhysRevD.93.082002
PG 8
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DI8SF
UT WOS:000373770800001
ER
PT J
AU Arzoumanian, Z
Brazier, A
Burke-Spolaor, S
Chamberlin, SJ
Chatterjee, S
Christy, B
Cordes, JM
Cornish, NJ
Crowter, K
Demorest, PB
Deng, X
Dolch, T
Ellis, JA
Ferdman, RD
Fonseca, E
Garver-Daniels, N
Gonzalez, ME
Jenet, F
Jones, G
Jones, ML
Kaspi, VM
Koop, M
Lam, MT
Lazio, TJW
Levin, L
Lommen, AN
Lorimer, DR
Luo, J
Lynch, RS
Madison, DR
McLaughlin, MA
McWilliams, ST
Mingarelli, CMF
Nice, DJ
Palliyaguru, N
Pennucci, TT
Ransom, SM
Sampson, L
Sanidas, SA
Sesana, A
Siemens, X
Simon, J
Stairs, IH
Stinebring, DR
Stovall, K
Swiggum, J
Taylor, SR
Vallisneri, M
van Haasteren, R
Wang, Y
Zhu, WW
AF Arzoumanian, Z.
Brazier, A.
Burke-Spolaor, S.
Chamberlin, S. J.
Chatterjee, S.
Christy, B.
Cordes, J. M.
Cornish, N. J.
Crowter, K.
Demorest, P. B.
Deng, X.
Dolch, T.
Ellis, J. A.
Ferdman, R. D.
Fonseca, E.
Garver-Daniels, N.
Gonzalez, M. E.
Jenet, F.
Jones, G.
Jones, M. L.
Kaspi, V. M.
Koop, M.
Lam, M. T.
Lazio, T. J. W.
Levin, L.
Lommen, A. N.
Lorimer, D. R.
Luo, J.
Lynch, R. S.
Madison, D. R.
McLaughlin, M. A.
McWilliams, S. T.
Mingarelli, C. M. F.
Nice, D. J.
Palliyaguru, N.
Pennucci, T. T.
Ransom, S. M.
Sampson, L.
Sanidas, S. A.
Sesana, A.
Siemens, X.
Simon, J.
Stairs, I. H.
Stinebring, D. R.
Stovall, K.
Swiggum, J.
Taylor, S. R.
Vallisneri, M.
van Haasteren, R.
Wang, Y.
Zhu, W. W.
CA NANOGrav Collaboration
TI THE NANOGRAV NINE-YEAR DATA SET: LIMITS ON THE ISOTROPIC STOCHASTIC
GRAVITATIONAL WAVE BACKGROUND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational waves; methods data analysis; pulsars general
ID BLACK-HOLE BINARIES; PULSAR TIMING ARRAYS; ACTIVE GALACTIC NUCLEI;
MILLISECOND PULSARS; BRANE INFLATION; COSMIC STRINGS; STELLAR MASS; NGC
1277; EVOLUTION; RADIATION
AB We compute upper limits on the nanohertz-frequency isotropic stochastic gravitational wave background (GWB) using the 9 year data set from the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) collaboration. Well-tested Bayesian techniques are used to set upper limits on the dimensionless strain amplitude (at a frequency of 1 yr(-1)) for a GWB from supermassive black hole binaries of A(gw) < 1.5 x 10(-15). We also parameterize the GWB spectrum with a broken power-law model by placing priors on the strain amplitude derived from simulations of Sesana and McWilliams et al. Using Bayesian model selection we find that the data favor a broken power law to a pure power law with odds ratios of 2.2 and 22 to one for the Sesana and McWilliams prior models, respectively. Using the broken power-law analysis we construct posterior distributions on environmental factors that drive the binary to the GW-driven regime including the stellar mass density for stellar-scattering, mass accretion rate for circumbinary disk interaction, and orbital eccentricity for eccentric binaries, marking the first time that the shape of the GWB spectrum has been used to make astrophysical inferences. Returning to a power-law model, we place stringent limits on the energy density of relic GWs, Omega(gw) (f)h(2) < 4.2 x 10(-10). Our limit on the cosmic string GWB, Omega(gw) (f)h(2) < 2.2 x 10(-10), translates to a conservative limit on the cosmic string tension with G mu < 3.3 x 10(-8), a factor of four better than the joint Planck and high-l cosmic microwave background data from other experiments.
C1 [Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Brazier, A.; Chatterjee, S.; Cordes, J. M.; Dolch, T.; Lam, M. T.; Madison, D. R.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Burke-Spolaor, S.; Demorest, P. B.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Chamberlin, S. J.; Deng, X.; Koop, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Christy, B.; Lommen, A. N.] Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA.
[Cornish, N. J.; Sampson, L.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
[Crowter, K.; Fonseca, E.; Gonzalez, M. E.; Stairs, I. H.; Zhu, W. W.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Dolch, T.] Hillsdale Coll, Dept Phys, Hillsdale, MI 49242 USA.
[Ellis, J. A.; Lazio, T. J. W.; Taylor, S. R.; Vallisneri, M.; van Haasteren, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ferdman, R. D.; Kaspi, V. M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Garver-Daniels, N.; Jones, M. L.; Levin, L.; Lorimer, D. R.; McLaughlin, M. A.; McWilliams, S. T.; Palliyaguru, N.; Swiggum, J.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
[Gonzalez, M. E.] Vancouver Coastal Hlth Author, Dept Nucl Med, Vancouver, BC V5Z 1M9, Canada.
[Jenet, F.; Luo, J.] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA.
[Jones, G.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Lynch, R. S.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Madison, D. R.; Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Mingarelli, C. M. F.] CALTECH, TAPIR, Pasadena, CA 91125 USA.
[Mingarelli, C. M. F.; Zhu, W. W.] Max Planck Inst Radio Astron, D-53121 Bonn, Germany.
[Nice, D. J.] Lafayette Coll, Dept Phys, Easton, PA 18042 USA.
[Pennucci, T. T.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Sanidas, S. A.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Sanidas, S. A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Sesana, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Siemens, X.; Simon, J.] Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA.
[Stinebring, D. R.] Oberlin Coll, Dept Phys & Astron, Oberlin, OH 44074 USA.
[Stovall, K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
[Wang, Y.] Huazhong Univ Sci & Technol, Sch Phys, Wuhan 430074, Hubei Province, Peoples R China.
RP Ellis, JA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Justin.A.Ellis@jpl.nasa.gov
OI Taylor, Stephen/0000-0003-0264-1453
FU National Science Foundation (NSF) PIRE program [0968296]; NSF Physics
Frontier Center [1430284]; NSERC Discovery Grant; Discovery Accelerator
Supplement; Canadian Institute for Advanced Research; JPL RTD program;
Marie Curie International Outgoing Fellowship within 7th European
Community Framework Programme; NASA Postdoctoral Program at the Jet
Propulsion Laboratory; NASA through Einstein Fellowship [PF4-150120,
PF3-140116]; NWO Vidi fellowship; University Research Fellowship of the
Royal Society; National Science Foundation of China (NSFC) [11503007];
National Science Foundation [PHYS-1066293]; NSF [MRI-R2, PHY-0960291,
0923409]; Sherman Fairchild Foundation
FX We would like to thank David Merritt for his useful comments on the
manuscript. The NANOGrav project receives support from National Science
Foundation (NSF) PIRE program award number 0968296 and NSF Physics
Frontier Center award number 1430284. NANOGrav research at UBC is
supported by an NSERC Discovery Grant and Discovery Accelerator
Supplement and by the Canadian Institute for Advanced Research. D.R.M.
acknowledges partial support through the New York Space Grant
Consortium. M.V. acknowledges support from the JPL RTD program. Portions
of this research were carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. C.M.F.M. was supported by a Marie
Curie International Outgoing Fellowship within the 7th European
Community Framework Programme. S.R.T. was supported by appointment to
the NASA Postdoctoral Program at the Jet Propulsion Laboratory,
administered by Oak Ridge Associated Universities through a contract
with NASA. J.A.E. and Rv.H. acknowledge support by NASA through Einstein
Fellowship grants PF4-150120 and PF3-140116, respectively. S.A.S.
acknowledges funding from an NWO Vidi fellowship (PI: JTW Hessels). A.
S. is supported by a University Research Fellowship of the Royal
Society. Y.W. is supported by the National Science Foundation of China
(NSFC) under grant NO. 11503007. This work was supported in part by
National Science Foundation Grant No. PHYS-1066293 and by the
hospitality of the Aspen Center for Physics. This research was performed
in part using the Zwicky computer cluster at Caltech supported by NSF
under MRI-R2 award no. PHY-0960291 and by the Sherman Fairchild
Foundation. A majority of the computational work was performed on the
Nemo cluster at UWM supported by NSF grant No. 0923409. Parts of the
analysis in this work were carried out on the Nimrod cluster made
available by S.M.R. Data for this project were collected using the
facilities of the National Radio Astronomy Observatory and the Arecibo
Observatory. The National Radio Astronomy Observatory is a facility of
the NSF operated under cooperative agreement by Associated Universities,
Inc. The Arecibo Observatory is operated by SRI International under a
cooperative agreement with the NSF (AST-1100968), and in alliance with
Ana G. Mendez-Universidad Metropolitana and the Universities Space
Research Association.
NR 122
TC 23
Z9 23
U1 2
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 13
DI 10.3847/0004-637X/821/1/13
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000013
ER
PT J
AU Bradshaw, SJ
Viall, NM
AF Bradshaw, S. J.
Viall, N. M.
TI PATTERNS OF ACTIVITY IN A GLOBAL MODEL OF A SOLAR ACTIVE REGION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: transition region; Sun: UV radiation
ID X-RAY TELESCOPE; CORONAL LOOPS; HOT PLASMA; CHROMOSPHERIC NANOFLARES;
EMISSION MEASURE; TIME-DEPENDENCE; ATOMIC DATABASE; MAGNETIC LOOPS;
HEATING MODEL; DYNAMICS
AB In this work we investigate the global activity patterns predicted from a model active region heated by distributions of nanoflares that have a range of frequencies. What differs is the average frequency of the distributions. The activity patterns are manifested in time lag maps of narrow-band instrument channel pairs. We combine hydrodynamic and forward modeling codes with a magnetic field extrapolation to create a model active region and apply the time lag method to synthetic observations. Our aim is not to reproduce a particular set of observations in detail, but to recover some typical properties and patterns observed in active regions. Our key findings are the following. (1) Cooling dominates the time lag signature and the time lags between the channel pairs are generally consistent with observed values. (2) Shorter coronal loops in the core cool more quickly than longer loops at the periphery. (3) All channel pairs show zero time lag when the line of sight passes through coronal loop footpoints. (4) There is strong evidence that plasma must be re-energized on a timescale comparable to the cooling timescale to reproduce the observed coronal activity, but it is likely that a relatively broad spectrum of heating frequencies are operating across active regions. (5) Due to their highly dynamic nature, we find nanoflare trains produce zero time lags along entire flux tubes in our model active region that are seen between the same channel pairs in observed active regions.
C1 [Bradshaw, S. J.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
[Viall, N. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Bradshaw, SJ (reprint author), Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.; Viall, NM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM stephen.bradshaw@rice.edu; Nicholeen.M.Viall@nasa.gov
OI Viall, Nicholeen/0000-0003-1692-1704
FU NSF [AGS-1450230]; NASA
FX S.J.B. is grateful to the NSF for supporting this work through CAREER
award AGS-1450230 and N.M.V. is grateful to NASA through the GI program.
The authors benefited from participating in the team hosted by the
International Space Science Institute, Bern, on Using Observables to
Settle the Question of Steady versus Impulsive Coronal Heating, led by
S.J.B. and Helen Mason. The authors also thank Dr. Jim Klimchuk and the
referee for their helpful comments on the manuscript.
NR 61
TC 2
Z9 2
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 63
DI 10.3847/0004-637X/821/1/63
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000063
ER
PT J
AU Chhiber, R
Usmanov, AV
Matthaeus, WH
Goldstein, ML
AF Chhiber, R.
Usmanov, A. V.
Matthaeus, W. H.
Goldstein, M. L.
TI SOLAR WIND COLLISIONAL AGE FROM A GLOBAL MAGNETOHYDRODYNAMICS SIMULATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); methods: numerical; plasmas; scattering;
Solar wind; Turbulence
ID COULOMB COLLISIONS; 3-DIMENSIONAL MODEL; COROTATING STREAMS; MHD MODEL;
PLASMAS; FLOW
AB Simple estimates of the number of Coulomb collisions experienced by the interplanetary plasma to the point of observation, i.e., the "collisional age", can be usefully employed in the study of non-thermal features of the solar wind. Usually these estimates are based on local plasma properties at the point of observation. Here we improve the method of estimation of the collisional age by employing solutions obtained from global three-dimensional magnetohydrodynamics simulations. This enables evaluation of the complete analytical expression for the collisional age without using approximations. The improved estimation of the collisional timescale is compared with turbulence and expansion timescales to assess the relative importance of collisions. The collisional age computed using the approximate formula employed in previous work is compared with the improved simulation-based calculations to examine the validity of the simplified formula. We also develop an analytical expression for the evaluation of the collisional age and we find good agreement between the numerical and analytical results. Finally, we briefly discuss the implications for an improved estimation of collisionality along spacecraft trajectories, including Solar Probe Plus.
C1 [Chhiber, R.; Usmanov, A. V.; Matthaeus, W. H.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Chhiber, R.; Usmanov, A. V.; Matthaeus, W. H.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Usmanov, A. V.; Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Chhiber, R (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.; Chhiber, R (reprint author), Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
OI GOLDSTEIN, MELVYN/0000-0002-5317-988X
FU Solar Probe Plus ISIS project; NSF [AGS-1156094, AGS-1063439]; LWS NASA
grant [NNX09AH79G]; Heliospheric Grand Challenge Research program
[NNX14AI63G]
FX This research was partially supported by the Solar Probe Plus ISIS
project; the NSF SHINE (AGS-1156094) and Solar Terrestrial (AGS-1063439)
programs; the LWS NASA grant NNX09AH79G; and the Heliospheric Grand
Challenge Research program (NNX14AI63G). We would like to thank the
referees for several useful suggestions that improved the paper.
NR 29
TC 1
Z9 1
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 34
DI 10.3847/0004-637X/821/1/34
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000034
ER
PT J
AU Drout, MR
Milisavljevic, D
Parrent, J
Margutti, R
Kamble, A
Soderberg, AM
Challis, P
Chornock, R
Fong, W
Frank, S
Gehrels, N
Graham, ML
Hsiao, E
Itagaki, K
Kasliwal, M
Kirshner, RP
Macomb, D
Marion, GH
Norris, J
Phillips, MM
AF Drout, M. R.
Milisavljevic, D.
Parrent, J.
Margutti, R.
Kamble, A.
Soderberg, A. M.
Challis, P.
Chornock, R.
Fong, W.
Frank, S.
Gehrels, N.
Graham, M. L.
Hsiao, E.
Itagaki, K.
Kasliwal, M.
Kirshner, R. P.
Macomb, D.
Marion, G. H.
Norris, J.
Phillips, M. M.
TI THE DOUBLE-PEAKED SN 2013ge: A TYPE Ib/c SN WITH AN ASYMMETRIC MASS
EJECTION OR AN EXTENDED PROGENITOR ENVELOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernovae: general; supernovae: individual (SN 2013ge)
ID CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY BURSTS; NEUTRINO-DRIVEN EXPLOSIONS;
RADIO OBSERVATIONS REVEAL; LIGHT CURVES; IA SUPERNOVAE; IBC SUPERNOVA;
IC SUPERNOVAE; SHOCK BREAKOUT; CASSIOPEIA-A
AB We present extensive multiwavelength (radio to X-ray) observations of the Type Ib/c supernova (SN Ib/c) SN 2013ge from -13 to +457 days relative to maximum light, including a series of optical spectra and Swift UV-optical photometry beginning 2-4 days post-explosion. This data set makes SN 2013ge one of the best-observed normal SNe Ib/c at early times-when the light curve is particularly sensitive to the progenitor configuration and mixing of radioactive elements-and reveals two distinct light curve components in the UV bands. The first component rises over 4-5 days and is visible for the first week post-explosion. Spectra of the first component have blue continua and show a plethora of moderately high. velocity (similar to 15,000 km s(-1)) but narrow (similar to 3500 km s(-1)) spectroscopic features, indicating that the line-forming region is restricted. The explosion parameters estimated for the bulk explosion (M-ej similar to 2-3 M-circle dot; E-K similar to (1-2) x 10(51) erg) are standard for SNe Ib/c, and there is evidence for weak He features at early times-in an object that. would have otherwise been classified as Type Ic. In addition, SN 2013ge exploded in a low-metallicity environment (similar to 0.5 Z(circle dot)), and we have obtained some of the deepest radio and X-ray limits for an SN Ib/c to date, which constrain the progenitor mass-loss rate to be (M) over dot < 4 x 10(-6) M-circle dot yr(-1). We are left with two distinct progenitor scenarios for SN 2013ge, depending on our interpretation of the early emission. If the first component is cooling envelope emission, then the progenitor of SN 2013ge either possessed an extended (greater than or similar to 30 R-circle dot) envelope or ejected a portion of its envelope in the final less than or similar to 1 yr before core. collapse. Alternatively, if the first component is due to outwardly mixed Ni-56, then our observations are consistent with the asymmetric ejection of a distinct clump of nickel-rich material at high velocities. Current models for the collision of an. SN. shock with a binary companion cannot reproduce both the timescale and luminosity of the early emission in SN 2013ge. Finally, the spectra of the first component of SN 2013ge are similar to those of the rapidly declining SN 2002bj.
C1 [Drout, M. R.; Milisavljevic, D.; Parrent, J.; Margutti, R.; Kamble, A.; Soderberg, A. M.; Challis, P.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chornock, R.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Clippinger Lab 251B, Athens, OH 45701 USA.
[Fong, W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Frank, S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Graham, M. L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Hsiao, E.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Hsiao, E.; Phillips, M. M.] Las Campanas Observ, Carnegie Observ, Colina El Pino, Chile.
[Itagaki, K.] Itagaki Astron Observ, Yamagata, Yamagata 9902492, Japan.
[Kasliwal, M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Macomb, D.; Norris, J.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Drout, MR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mdrout@cfa.harvard.edu
OI Parrent, Jerod/0000-0002-5103-7706; Margutti,
Raffaella/0000-0003-4768-7586
FU NSF Graduate Research Fellowship; Gary and Cynthia Bengier; NSF
[AST-1211916, AST-9987045]; Danish Agency for Science and Technology and
Innovation through a Sapere Aude Level 2 grant; NSF Telescope System
Instrumentation Program (TSIP); Ohio Board of Regents; Ohio State
University Office of Research
FX We thank the anonymous referee for numerous comments that improved this
manuscript. M.R.D. thanks L. Z. Kelley, D. Kasen, and E. Ramirez-Ruiz
for useful discussions. We thank N. Morrell for obtaining some of the
observations reported here. M.R.D. is supported in part by the NSF
Graduate Research Fellowship. M.L.G.'s position in the supernova
research group at UC Berkeley is supported by Gary and Cynthia Bengier
and NSF grant AST-1211916. E.Y.H. acknowledges the generous support
provided by the Danish Agency for Science and Technology and Innovation
through a Sapere Aude Level 2 grant.; This paper includes data gathered
with the 6.5 m Magellan Telescopes located at Las Campanas Observatory,
Chile. Some observations reported here were obtained at the MMT
observatory, a joint facility of the Smithsonian Institution and the
University of Arizona. This paper uses data taken with the MODS
spectrographs built with funding from NSF grant AST-9987045 and the NSF
Telescope System Instrumentation Program (TSIP), with additional funds
from the Ohio Board of Regents and the Ohio State University Office of
Research.
NR 160
TC 1
Z9 1
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 57
DI 10.3847/0004-637X/821/1/57
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000057
ER
PT J
AU Fausnaugh, MM
Denney, KD
Barth, AJ
Bentz, MC
Bottorff, MC
Carini, MT
Croxall, KV
De Rosa, G
Goad, MR
Horne, K
Joner, MD
Kaspi, S
Kim, M
Klimanov, SA
Kochanek, CS
Leonard, DC
Netzer, H
Peterson, BM
Schnulle, K
Sergeev, SG
Vestergaard, M
Zheng, WK
Zu, Y
Anderson, MD
Arevalo, P
Bazhaw, C
Borman, GA
Boroson, TA
Brandt, WN
Breeveld, AA
Brewer, BJ
Cackett, EM
Crenshaw, DM
Dalla Bonta, E
De Lorenzo-Caceres, A
Dietrich, M
Edelson, R
Efimova, NV
Ely, J
Evans, PA
Filippenko, AV
Flatland, K
Gehrels, N
Geier, S
Gelbord, JM
Gonzalez, L
Gorjian, V
Grier, CJ
Grupe, D
Hall, PB
Hicks, S
Horenstein, D
Hutchison, T
Im, M
Jensen, JJ
Jones, J
Kaastra, J
Kelly, BC
Kennea, JA
Kim, SC
Korista, KT
Kriss, GA
Lee, JC
Lira, P
MacInnis, F
Manne-Nicholas, ER
Mathur, S
McHardy, IM
Montouri, C
Musso, R
Nazarov, SV
Norris, RP
Nousek, JA
Okhmat, DN
Pancoast, A
Papadakis, I
Parks, JR
Pei, L
Pogge, RW
Pott, JU
Rafter, SE
Rix, HW
Saylor, DA
Schimoia, JS
Siegel, M
Spencer, M
Starkey, D
Sung, HI
Teems, KG
Treu, T
Turner, CS
Uttley, P
Villforth, C
Weiss, Y
Woo, JH
Yan, H
Young, S
AF Fausnaugh, M. M.
Denney, K. D.
Barth, A. J.
Bentz, M. C.
Bottorff, M. C.
Carini, M. T.
Croxall, K. V.
De Rosa, G.
Goad, M. R.
Horne, Keith
Joner, M. D.
Kaspi, S.
Kim, M.
Klimanov, S. A.
Kochanek, C. S.
Leonard, D. C.
Netzer, H.
Peterson, B. M.
Schnuelle, K.
Sergeev, S. G.
Vestergaard, M.
Zheng, W. -K.
Zu, Y.
Anderson, M. D.
Arevalo, P.
Bazhaw, C.
Borman, G. A.
Boroson, T. A.
Brandt, W. N.
Breeveld, A. A.
Brewer, B. J.
Cackett, E. M.
Crenshaw, D. M.
Dalla Bonta, E.
De Lorenzo-Caceres, A.
Dietrich, M.
Edelson, R.
Efimova, N. V.
Ely, J.
Evans, P. A.
Filippenko, A. V.
Flatland, K.
Gehrels, N.
Geier, S.
Gelbord, J. M.
Gonzalez, L.
Gorjian, V.
Grier, C. J.
Grupe, D.
Hall, P. B.
Hicks, S.
Horenstein, D.
Hutchison, T.
Im, M.
Jensen, J. J.
Jones, J.
Kaastra, J.
Kelly, B. C.
Kennea, J. A.
Kim, S. C.
Korista, K. T.
Kriss, G. A.
Lee, J. C.
Lira, P.
MacInnis, F.
Manne-Nicholas, E. R.
Mathur, S.
McHardy, I. M.
Montouri, C.
Musso, R.
Nazarov, S. V.
Norris, R. P.
Nousek, J. A.
Okhmat, D. N.
Pancoast, A.
Papadakis, I.
Parks, J. R.
Pei, L.
Pogge, R. W.
Pott, J. -U.
Rafter, S. E.
Rix, H. -W.
Saylor, D. A.
Schimoia, J. S.
Siegel, M.
Spencer, M.
Starkey, D.
Sung, H. -I.
Teems, K. G.
Treu, T.
Turner, C. S.
Uttley, P.
Villforth, C.
Weiss, Y.
Woo, J. -H.
Yan, H.
Young, S.
TI SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. III. OPTICAL
CONTINUUM EMISSION AND BROADBAND TIME DELAYS IN NGC 5548
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 5548); galaxies: nuclei;
galaxies: Seyfert
ID ACTIVE GALACTIC NUCLEI; AGN MONITORING PROJECT; DIGITAL SKY SURVEY;
DAMPED RANDOM-WALK; BLACK-HOLE MASSES; COSMIC ORIGINS SPECTROGRAPH;
QUASI-STELLAR OBJECTS; DRIVEN DISK WINDS; LINE REGION; X-RAY
AB We present ground-based optical photometric monitoring data for NGC 5548, part of an extended multiwavelength reverberation mapping campaign. The light curves have nearly daily cadence from 2014 January to July in nine filters (BVRI and ugriz). Combined with ultraviolet data from the Hubble Space Telescope and Swift, we confirm significant time delays between the continuum bands as a function of wavelength, extending the wavelength coverage from 1158 angstrom to the z band (similar to 9160 angstrom). We find that the lags at wavelengths longer than the V band are equal to or greater than the lags of high-ionization-state emission lines (such as He II lambda 1640 and lambda 4686), suggesting that the continuum-emitting source is of a physical size comparable to the inner broad-line region (BLR). The trend of lag with wavelength is broadly consistent with the prediction for continuum reprocessing by an accretion disk with tau proportional to lambda(4/3). However, the lags also imply a disk radius that is 3 times larger than the prediction from standard thin-disk theory, assuming that the bolometric luminosity is 10% of the Eddington luminosity (L = 0.1L(Edd)). Using optical spectra from the Large Binocular Telescope, we estimate the bias of the interband continuum lags due to BLR emission observed in the filters. We find that the bias for filters with high levels of BLR contamination (similar to 20%) can be important for the shortest continuum lags. and likely has a significant impact on the u and U bands owing to Balmer continuum emission.
C1 [Fausnaugh, M. M.; Denney, K. D.; Croxall, K. V.; De Rosa, G.; Kochanek, C. S.; Peterson, B. M.; Zu, Y.; Grier, C. J.; Mathur, S.; Pogge, R. W.; Schimoia, J. S.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
[Denney, K. D.; Croxall, K. V.; De Rosa, G.; Kochanek, C. S.; Peterson, B. M.; Mathur, S.; Pogge, R. W.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA.
[Barth, A. J.; Pei, L.] Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA.
[Bentz, M. C.; Anderson, M. D.; Bazhaw, C.; Crenshaw, D. M.; Horenstein, D.; Jones, J.; Manne-Nicholas, E. R.; Norris, R. P.; Parks, J. R.; Saylor, D. A.; Teems, K. G.; Turner, C. S.] Georgia State Univ, Dept Phys & Astron, 25 Pk Pl,Suite 605, Atlanta, GA 30303 USA.
[Bottorff, M. C.; Hutchison, T.; MacInnis, F.; Musso, R.] Southwestern Univ, Dept Phys FJS 149, Fountainwood Observ, 1011 E Univ Ave, Georgetown, TX 78626 USA.
Western Kentucky Univ, Dept Phys & Astron, 1906 Coll Hts Blvd 11077, Bowling Green, KY 42101 USA.
[De Rosa, G.; Ely, J.; Kriss, G. A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Goad, M. R.; Evans, P. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Joner, M. D.; Spencer, M.] Brigham Young Univ, Dept Phys & Astron, N283 ESC, Provo, UT 84602 USA.
[Kaspi, S.; Netzer, H.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Kaspi, S.; Rafter, S. E.; Weiss, Y.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
[Kim, M.; Kim, S. C.; Lee, J. C.; Sung, H. -I.] Korea Astron & Space Sci Inst, Seoul, South Korea.
[Klimanov, S. A.; Efimova, N. V.] Pulkovo Observ, St Petersburg 196140, Russia.
San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Schnuelle, K.; Pott, J. -U.; Rix, H. -W.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Sergeev, S. G.; Borman, G. A.; Nazarov, S. V.; Okhmat, D. N.] Crimean Astrophys Observ, P-O Nauchny, Crimea 298409, Russia.
[Vestergaard, M.; Jensen, J. J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark.
[Vestergaard, M.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Zheng, W. -K.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
[Zu, Y.] Carnegie Mellon Univ, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.
[Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Gran Bretana N 1111, Valparaiso, Chile.
[Boroson, T. A.; Kennea, J. A.; Siegel, M.] Las Cumbres Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
[Brandt, W. N.; Grier, C. J.; Nousek, J. A.] Penn State Univ, Eberly Coll Sci, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Brandt, W. N.; Grier, C. J.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA.
[Breeveld, A. A.] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
[Brewer, B. J.] Univ Auckland, Dept Stat, Private Bag 92019, Auckland 1142, New Zealand.
[Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, 666 W Hancock St, Detroit, MI 48201 USA.
[Dalla Bonta, E.] Univ Padua, Dipartimento Fis & Astron G Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy.
[Dalla Bonta, E.] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy.
[Dietrich, M.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
[Dietrich, M.] Worcester State Univ, Dept Earth Environm & Phys, 486 Chandler St, Worcester, MA 01602 USA.
[Edelson, R.; Young, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Geier, S.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain.
[Geier, S.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Geier, S.] Gran Telescopio Canarias GRANTECAN, E-38205 Tenerife, Spain.
[Gelbord, J. M.] Spectral Sci Inc, 4 Fourth Ave, Burlington, MA 01803 USA.
[Gelbord, J. M.] Eureka Sci Inc, 2452 Delmer St,Suite 100, Oakland, CA 94602 USA.
[Gorjian, V.] CALTECH, Jet Prop Lab, MS 169-327,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Grupe, D.] Morehead State Univ, Ctr Space Sci, 235 Martindale Dr, Morehead, KY 40351 USA.
[Hall, P. B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Im, M.; Woo, J. -H.] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul, South Korea.
[Kaastra, J.] SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CC Utrecht, Netherlands.
[Kaastra, J.] Univ Utrecht, Dept Phys & Astron, POB 80000, NL-3508 Utrecht, Netherlands.
[Kaastra, J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Kelly, B. C.; Treu, T.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Korista, K. T.] Western Michigan Univ, Dept Phys, 1120 Everett Tower, Kalamazoo, MI 49008 USA.
[Kriss, G. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lira, P.] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile.
[McHardy, I. M.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Montouri, C.] Univ Insubria, DiSAT, Via Valleggio 11, I-22100 Como, Italy.
[Pancoast, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Papadakis, I.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece.
[Papadakis, I.] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Greece.
[Papadakis, I.] Fdn Res & Technol, IESL, GR-71110 Iraklion, Greece.
[Rafter, S. E.] Univ Haifa, Fac Nat Sci, Dept Phys, IL-31905 Haifa, Israel.
[Schimoia, J. S.] Univ Fed Rio Grande do Sul, Inst Fis, Campus Vale, Porto Alegre, RS, Brazil.
[Treu, T.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Uttley, P.] Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands.
[Villforth, C.] Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England.
[Yan, H.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
RP Fausnaugh, MM (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
RI Lira, Paulina/G-8536-2016; Papadakis, Iossif/C-3235-2011;
OI Zu, Ying/0000-0001-6966-6925; Vestergaard, Marianne/0000-0001-9191-9837;
Im, Myungshin/0000-0002-8537-6714; Barth, Aaron/0000-0002-3026-0562
FU National Science Foundation (NSF) [AST-9987045]; NSF [AST-1108693,
AST-1008882, AST-1412693, AST-1211916, AST-1302093, AST-0618209,
AST-1009756, AST-1009571, AST-1210311, AST-1412315]; Ohio Board of
Regents; Ohio State University Office of Research; UK Science and
Technology Facilities Council; NASA through Space Telescope Science
Institute [GO-13330]; NASA [NAS5-26555, NNX13AC26G, NNX13AC63G,
NNX13AE99G, NNH13CH61C]; TABASGO Foundation; Christopher R. Redlich
Fund; NSF CAREER grant [AST-1253702]; HHMI; NSERC; Creative Initiative
program of the National Research Foundation of Korea (NRFK) - Korean
government (MSIP) [2008-0060544]; NWO, the Netherlands Organization for
Scientific Research; UC Center for Galaxy Evolution; Fondecyt [1120328];
UCSB Dean's Fellowship; NASA Einstein Fellowship; CNPq, National Council
for Scientific and Technological Development (Brazil); Packard
Foundation; Danish National Research Foundation; Danish Council for
Independent Research [DFF-400200275]; National Research Foundation of
Korea (NRF) grant - Korean government [2010-0027910]; Padua University
[60A02-5857/13, 60A02-5833/14, 60A02-4434/15, CPDA133894]; STFC grant
[ST/M001296/1]
FX This paper used data obtained with the MODS spectrographs built with
funding from National Science Foundation (NSF) grant AST-9987045 and the
NSF Telescope System Instrumentation Program (TSIP), with additional
funds from the Ohio Board of Regents and the Ohio State University
Office of Research. This paper made use of the mods IDL spectral data
reduction pipeline developed in part with funds provided by NSF Grant
AST-1108693.; The Liverpool Telescope is operated on the island of La
Palma by Liverpool John Moores University in the Spanish Observatorio
del Roque de los Muchachos of the Instituto de Astrofisica de Canarias
with financial support from the UK Science and Technology Facilities
Council.; Support for HST program number GO-13330 was provided by NASA
through a grant from the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS5-26555. M.M.F., G.D.R., B.M.P., C.J.G.,
and R.W.P. are grateful for the support of the NSF through grant
AST-1008882 to The Ohio State University. A.J.B. and L.P. have been
supported by NSF grant AST-1412693. A.V.F. and W.-K.Z. are grateful for
financial assistance from NSF grant AST-1211916, the TABASGO Foundation,
and the Christopher R. Redlich Fund. M.C. Bentz gratefully acknowledges
support through NSF CAREER grant AST-1253702 to Georgia State
University. M.C. Bottorff acknowledges HHMI for support through an
undergraduate science education grant to Southwestern University. K.D.D.
is supported by an NSF Fellowship awarded under grant AST-1302093. R.E.
gratefully acknowledges support from NASA under awards NNX13AC26G,
NNX13AC63G, and NNX13AE99G. J.M.G. gratefully acknowledges support from
NASA under award NNH13CH61C. P.B.H. is supported by NSERC. M.I.
acknowledges support from the Creative Initiative program, No.
2008-0060544, of the National Research Foundation of Korea (NRFK) funded
by the Korean government (MSIP). M.D.J. acknowledges NSF grant
AST-0618209 used for obtaining the 0.91 m telescope at WMO. SRON is
financially supported by NWO, the Netherlands Organization for
Scientific Research. B.C.K. is partially supported by the UC Center for
Galaxy Evolution. C.S.K. acknowledges the support of NSF grant
AST-1009756. D.C.L. acknowledges support from NSF grants AST-1009571 and
AST-1210311, under which part of this research (photometric observations
collected at MLO) was carried out. We thank Nhieu Duong, Harish
Khandrika, Richard Mellinger, J. Chuck Horst, Steven Armen, and Eddie
Garcia for assistance with the MLO observations. P.L. acknowledges
support from Fondecyt grant # 1120328. A.P. acknowledges support from an
NSF graduate fellowship, a UCSB Dean's Fellowship, and a NASA Einstein
Fellowship. J. S.S. acknowledges CNPq, National Council for Scientific
and Technological Development (Brazil) for partial support and The Ohio
State University for warm hospitality. T.T. has been supported by NSF
grant AST-1412315. T.T. and B.C.K. acknowledge support from the Packard
Foundation in the form of a Packard Research Fellowship to T.T.; also,
T.T. thanks the American Academy in Rome and the Observatory of
Monteporzio Catone for kind hospitality. The Dark Cosmology Centre is
funded by the Danish National Research Foundation. M.V. gratefully
acknowledges support from the Danish Council for Independent Research
via grant no. DFF-400200275. J.-H.W. acknowledges support by the
National Research Foundation of Korea (NRF) grant funded by the Korean
government (No. 2010-0027910). E.D.B. is supported by Padua University
through grants 60A02-5857/13, 60A02-5833/14, 60A02-4434/15, and
CPDA133894. K.H. acknowledges support from STFC grant ST/M001296/1.
S.A.K. thanks Dr. I. A. Rakhimov, the director of Svetloe Observatory,
for his support and hospitality.
NR 113
TC 16
Z9 16
U1 7
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 56
DI 10.3847/0004-637X/821/1/56
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000056
ER
PT J
AU Kataria, T
Sing, DK
Lewis, NK
Visscher, C
Showman, AP
Fortney, JJ
Marley, MS
AF Kataria, Tiffany
Sing, David K.
Lewis, Nikole K.
Visscher, Channon
Showman, Adam P.
Fortney, Jonathan J.
Marley, Mark S.
TI THE ATMOSPHERIC CIRCULATION OF A NINE-HOT-JUPITER SAMPLE: PROBING
CIRCULATION AND CHEMISTRY OVER A WIDE PHASE SPACE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atmospheric effects; methods: numerical; planets and satellites: general
ID EXOPLANET HD 189733B; TRANSMISSION SPECTRAL SURVEY; TIDALLY LOCKED
EXOPLANETS; HOT JUPITER ATMOSPHERES; MU-M; CARBON-MONOXIDE; THERMAL
INVERSION; ORBITAL MOTION; MAGNETIC DRAG; GIANT PLANETS
AB We present results from an atmospheric circulation study of nine hot Jupiters that compose a large transmission spectral survey using the Hubble and Spitzer Space Telescopes. These observations exhibit a range of spectral behavior over optical and infrared wavelengths, suggesting diverse cloud and haze properties in their atmospheres. By utilizing the specific system parameters for each planet, we naturally probe a wide phase space in planet radius, gravity, orbital period, and equilibrium temperature. First, we show that our model "grid" recovers trends shown in traditional parametric studies of hot Jupiters, particularly equatorial superrotation and increased day-night temperature contrast with increasing equilibrium temperature. We show how spatial temperature variations, particularly between the dayside and nightside and west and east terminators, can vary by hundreds of kelvin, which could imply large variations in Na, K, CO and CH4 abundances in those regions. These chemical variations can be large enough to be observed in transmission with high-resolution spectrographs, such as ESPRESSO on VLT, METIS on the E-ELT, or. MIRI and NIRSpec aboard JWST. We also compare theoretical emission spectra generated from our models to. available Spitzer eclipse depths for each planet. and find that the outputs from our solar-metallicity, cloud-free models generally provide a good match to many of the data. sets, even without additional model tuning. Although these models are cloud-free, we can use their results to understand the chemistry and dynamics that drive cloud formation in their atmospheres.
C1 [Kataria, Tiffany; Sing, David K.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England.
[Lewis, Nikole K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Visscher, Channon] Dordt Coll, Dept Chem, Sioux Ctr, IA 51250 USA.
[Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Marley, Mark S.] NASA, Ames Res Ctr 245 3, Moffett Field, CA 94035 USA.
RP Kataria, T (reprint author), Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England.
EM tkataria@astro.ex.ac.uk
OI Marley, Mark/0000-0002-5251-2943
FU European Research Council under the European Unions Seventh Framework
Program/ERC grant [336792]; NASA program from STScI [HST-GO-12473]; BIS
National E-Infrastructure capital grant [ST/K000373/1]; STFC DiRAC
Operations grant [ST/K0003259/1]; NASA
FX We thank Caroline Morley, Nikolay Nikolov, Thomas Evans, and Hannah
Wakeford for useful discussions that. improved the manuscript. We also
acknowledge that part of this work was completed at the Space Telescope
Science Institute (STScI) operated by AURA, Inc. This work is based on
observations with the NASA/ESA HST, obtained at the STScI. This work is
also based in part on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. The
research leading to these results has received funding from the European
Research Council under the European Unions Seventh Framework Program
(FP7/2007-2013)/ERC grant agreement no. 336792. Support for this work
was provided by NASA through grants under the HST-GO-12473 program from
the STScI. This work used the DiRAC Complexity system, operated by the
University of Leicester IT Services, which forms part of the STFC DiRAC
HPC Facility (www.dirac.ac.uk). This equipment is funded by BIS National
E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations
grant ST/K0003259/1. DiRAC is part of the National E-Infrastructure. We
also thank the anonymous referee for comments that greatly improved the
paper.
NR 75
TC 8
Z9 8
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 9
DI 10.3847/0004-637X/821/1/9
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000009
ER
PT J
AU Kounkel, M
Megeath, ST
Poteet, CA
Fischer, WJ
Hartmann, L
AF Kounkel, M.
Megeath, S. T.
Poteet, C. A.
Fischer, W. J.
Hartmann, L.
TI AN HST SURVEY FOR 100-1000 au COMPANIONS AROUND YOUNG STELLAR OBJECTS IN
THE ORION MOLECULAR CLOUDS: EVIDENCE FOR ENVIRONMENTALLY DEPENDENT
MULTIPLICITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: visual; infrared: stars; ISM: individual (Orion A); stars:
formation; stars: protostars
ID STAR-FORMING REGIONS; SPACE-TELESCOPE SURVEY; LOW-MASS STARS; BINARY
STARS; NEBULA-CLUSTER; PROTOSTELLAR SYSTEMS; EMBEDDED PROTOSTARS;
TRAPEZIUM CLUSTER; VISUAL BINARIES; IMAGING SURVEY
AB We present a near-infrared survey for the visual multiples in the Orion molecular clouds region at separations between 100 and 1000 au. These data were acquired at 1.6 mu m with the NICMOS and WFC3 cameras on the Hubble Space Telescope. Additional photometry was obtained for some of the sources at 2.05 mu m with NICMOS and in the L' band with NSFCAM2 on NASA's InfraRed Telescope Facility. Toward 129 protostars and 197 premain-sequence stars with disks observed with WFC3, we detect 21 and 28 candidate companions between the projected separations of 100-1000 au, of which less than 5 and 8, respectively, are chance line-of-sight coincidences. The resulting companion fraction (CF) after the correction for the line-of-sight contamination is 14.4(-1.3)(+1.3)% for protostars and 12.5(-0.8)(+0.8)% for the pre-main-sequence stars. These values are similar to those found for main-sequence stars, suggesting that there is little variation in the CF with evolution, although several observational biases may mask a decrease in the CF from protostars to the main-sequence stars. After segregating the sample into two populations based on the surrounding surface density of young stellar objects, we find that the CF in the high stellar density regions (Sigma(YSO) > 45 pc(-2)) is approximately 50% higher than that found in the low stellar density regions (Sigma(YSO) < 45 pc(-2)). We interpret this as evidence for the elevated formation of companions at 100-1000 au in the denser environments of Orion. We discuss possible reasons for this elevated formation.
C1 [Kounkel, M.; Hartmann, L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA.
[Poteet, C. A.] Rensselaer Polytech Inst, New York Ctr Astrobiol, Troy, NY USA.
[Poteet, C. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Fischer, W. J.] NASA, Postdoctoral Program, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Kounkel, M (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
OI Fischer, William J/0000-0002-3747-2496; Kounkel,
Marina/0000-0002-5365-1267
FU NSF-REU program at the department of Physics and Astronomy at the
University of Toledo [PHY-1004649]; NASA through a grant from the Space
Telescope Science Institute [11548]; NASA [NAS 5-26555, NNX-08AE38A];
National Science Foundation
FX We acknowledge valuable conversations with John Tobin, Fred Adams, and
Mike Meyer. M.K. acknowledges support from the NSF-REU program at the
department of Physics and Astronomy at the University of Toledo (grant
PHY-1004649). We would also like to thank the anonymous referee and the
statistics editor of ApJ for valuable comments. Support for program
11548 was provided by NASA through a grant from the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS 5-26555. We
also used the Spitzer Space Telescope and the Infrared Processing and
Analysis Center (IPAC) Infrared Science Archive, which are operated by
JPL/Caltech under a contract with NASA. We also made use of the Infrared
Telescope Facility (IRTF), which is operated by the University of Hawaii
under Cooperative Agreement NNX-08AE38A with NASA, Science Mission
Directorate, Planetary Astronomy Program. The authors wish to recognize
and acknowledge the very significant cultural role and reverence that
the summit of Mauna Kea has always had within the indigenous Hawaiian
community. We are most fortunate to have the opportunity to conduct
observations from this mountain. This paper makes use of data products
from the Two Micron All Sky Survey, which is a joint project of the
University of Massachusetts and IPAC/Caltech, funded by NASA and the
National Science Foundation.
NR 68
TC 1
Z9 1
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 52
DI 10.3847/0004-637X/821/1/52
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000052
ER
PT J
AU Lam, MT
Cordes, JM
Chatterjee, S
Jones, ML
McLaughlin, MA
Armstrong, JW
AF Lam, M. T.
Cordes, J. M.
Chatterjee, S.
Jones, M. L.
McLaughlin, M. A.
Armstrong, J. W.
TI SYSTEMATIC AND STOCHASTIC VARIATIONS IN PULSAR DISPERSION MEASURES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: general; pulsars: general
ID THERMAL NOISE SPECTROSCOPY; ELECTRON-DENSITY MODEL; INTERSTELLAR-MEDIUM;
MILLISECOND PULSARS; RADIO PULSARS; REFRACTIVE SCINTILLATION; BOW SHOCK;
SCATTERING; PRECISION; B1937+21
AB We analyze deterministic and random temporal variations in the dispersion measure (DM) from the full three-dimensional velocities of pulsars with respect to the solar system, combined with electron-density variations over a wide range of length scales. Previous treatments have largely ignored pulsars' changing distances while favoring interpretations involving changes in sky position from transverse motion. Linear trends in pulsar DMs observed over 5-10 year timescales may signify sizable DM gradients in the interstellar medium (ISM) sampled by the changing direction of the line of sight to the pulsar. We show that motions parallel to the line of sight can also account for linear trends, for the apparent excess of DM variance over that extrapolated from scintillation measurements, and for the apparent non-Kolmogorov scalings of DM structure functions inferred in some cases. Pulsar motions through atomic gas may produce bow-shock ionized gas that also contributes to DM variations. We discuss the possible causes of periodic or quasi-periodic changes in DM, including seasonal changes in the ionosphere, annual variations of the solar elongation angle, structure in the heliosphere and ISM boundary, and substructure in the ISM. We assess the solar cycle's role on the amplitude of ionospheric and solar wind variations. Interstellar refraction can produce cyclic timing variations from the error in transforming arrival times to the solar system barycenter. We apply our methods to DM time series and DM gradient measurements in the literature and assess their consistency with a Kolmogorov medium. Finally, we discuss the implications of DM modeling in precision pulsar timing experiments.
C1 [Lam, M. T.; Cordes, J. M.; Chatterjee, S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Lam, M. T.; Cordes, J. M.; Chatterjee, S.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
[Jones, M. L.; McLaughlin, M. A.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
[Armstrong, J. W.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Lam, MT (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.; Lam, MT (reprint author), Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
EM mlam@astro.cornell.edu
FU NSF PIRE program [0968296]; NSF Physics Frontier Center [1430284]; NASA
New York Space Grant [NNX15AK07H]
FX Work on pulsar timing at Cornell University and West Virginia University
is supported in part by NSF PIRE program award number 0968296 and NSF
Physics Frontier Center award number 1430284. For J.W.A. the research
described here was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. M.T.L. was partially supported by
NASA New York Space Grant award number NNX15AK07H. We would like to
thank Merav Opher and Bertalan Zieger of Boston University for access to
their simulated heliosphere data. We thank Paul Demorest and Ryan
Shannon for data and assistance relating to PSR B1937+21, Emmanuel
Fonseca for data relating to PSR B1534+12, and Michael Keith for data
relating to PSRs J1909-3744, B1937 +21, and B1821-24. We would also like
to thank Bruno Nava for the source code to the NeQuick 2 model, David
Nice for assistance regarding solar wind modeling, John Antoniadis for
discussions on the 3D velocity of PSR J1909-3744, the NANOGrav ISM
Mitigation working group for useful conversations throughout the
duration of this project, and the anonymous referee for a very careful
readthrough of this work. We acknowledge NASA/GSFC's Space Physics Data
Facility's ftp service for Ulysses/SWOOPS
(http://spdf.sci.gsfc.nasa.gov/pub/data/ulysses/plasma/swoops/ion/hires/
data collection.
NR 77
TC 3
Z9 3
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 66
DI 10.3847/0004-637X/821/1/66
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000066
ER
PT J
AU Liu, HB
Lai, SP
Hasegawa, Y
Hirano, N
Rao, R
Li, IH
Fukagawa, M
Girart, JM
Carrasco-Gonzalez, C
Rodriguez, LF
AF Liu, Hauyu Baobab
Lai, Shih-Ping
Hasegawa, Yasuhiro
Hirano, Naomi
Rao, Ramprasad
Li, I-Hsiu
Fukagawa, Misato
Girart, Josep M.
Carrasco-Gonzalez, Carlos
Rodriguez, Luis F.
TI DETECTION OF LINEARLY POLARIZED 6.9 mm CONTINUUM EMISSION FROM THE CLASS
0 YOUNG STELLAR OBJECT NGC 1333 IRAS4A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE evolution; ISM: individual objects (NGC 1333 IRAS4A); stars: formation
ID UNDERSTANDING RADIO POLARIMETRY; PROTOSTELLAR DISK FORMATION;
MAGNETIC-FIELD STRUCTURE; STAR-FORMING CORES; KEPLERIAN DISK;
PROTOPLANETARY DISKS; MOLECULAR OUTFLOW; GRAIN ALIGNMENT; ENVELOPE; 4A
AB We report new Karl G. Jansky Very Large Array (JVLA), 0 ''.5 angular resolution observations of linearly polarized continuum emission at 6.9 mm, toward the class 0 young stellar object NGC 1333 IRAS4A. This target source is a collapsing dense molecular core that. was resolved at short wavelengths to have an hourglass shaped B-field configuration. We compare these 6.9 mm observations with previous polarization Submillimeter Array observations at 0.88 mm, which have a comparable angular resolution (similar to 0 ''.7). We find that at the same resolution, the observed polarization position angles at 6.9 mm are slightly deviated from those observed at 0.88 mm. Due to the lower optical depth of the emission at 6.9 mm, and the potential effect of dust grain growth, the new JVLA observations are likely probing B-field alignments in regions interior to those sampled by the previous polarization observations at higher frequencies. Our understanding can be improved with more sensitive observations, and with observations for the more extended spatial scales.
C1 [Liu, Hauyu Baobab; Hirano, Naomi; Rao, Ramprasad; Li, I-Hsiu] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan.
[Liu, Hauyu Baobab] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Lai, Shih-Ping] Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan.
[Lai, Shih-Ping] Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan.
[Hasegawa, Yasuhiro; Fukagawa, Misato] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Hasegawa, Yasuhiro] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Girart, Josep M.] CSIC IEEC, Inst Ciencies Espai, Campus UAB,Carrer de Can Magrans S-N, E-08193 Cerdanyola Del Valles, Catalonia, Spain.
[Girart, Josep M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Carrasco-Gonzalez, Carlos; Rodriguez, Luis F.] UNAM, Inst Radioastron & Astrofis, AP 3-72, Morelia 58089, Michoacan, Mexico.
RP Liu, HB (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan.; Liu, HB (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM hyliu@asiaa.sinica.edu.tw
OI Li, Jennifer/0000-0002-0311-2812; Girart, Josep
Miquel/0000-0002-3829-5591
FU ASIAA; MoST grant [104-2119-M-001-016]; MICINN (Spain)
[AYA2014-57369-C3-1-P]; MECD (Spain) [PRX15/00435]; UNAM-DGAPA-PAPIIT
[IA101214]; JPL/Caltech
FX H.B.L. is grateful for support from ASIAA. We are extremely grateful to
our referee Charles Hull,for the very useful comments. H.B.L. thanks Dr.
Steve Myers for the information about polarization calibration sources,
and thanks Drs. Akimasa Kataoka, Francisca Kemper, Hiroyuki Hirashita,
and Michihiro Takami for useful suggestions. N.H. is supported by the
MoST grant 104-2119-M-001-016. J.M.G. acknowledges support from the
MICINN (Spain) AYA2014-57369-C3-1-P grant and the MECD (Spain)
PRX15/00435 travel grant. C.C.-G. acknowledges support by
UNAM-DGAPA-PAPIIT, grant number IA101214. Y.H. is currently supported by
JPL/Caltech.
NR 52
TC 3
Z9 3
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 41
DI 10.3847/0004-637X/821/1/41
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000041
ER
PT J
AU Lohfink, AM
Reynolds, CS
Pinto, C
Alston, W
Boggs, SE
Christensen, FE
Craig, WW
Fabian, AC
Hailey, CJ
Harrison, FA
Kara, E
Matt, G
Parker, ML
Stern, D
Walton, D
Zhang, WW
AF Lohfink, A. M.
Reynolds, C. S.
Pinto, C.
Alston, W.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Fabian, A. C.
Hailey, C. J.
Harrison, F. A.
Kara, E.
Matt, G.
Parker, M. L.
Stern, D.
Walton, D.
Zhang, W. W.
TI THE RHYTHM OF FAIRALL 9. I. OBSERVING THE SPECTRAL VARIABILITY WITH
XMM-NEWTON AND NuSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; X-rays: individual (Fairall 9)
ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; X-RAY EXCESS; SUZAKU
OBSERVATIONS; NGC 5548; SWIFT; DISC; AGN; SPECTROSCOPY; TELESCOPE
AB We present a multi-epoch X-ray spectral analysis of the Seyfert. 1 galaxy Fairall. 9. Our analysis shows that Fairall. 9 displays unique spectral variability in that its ratio residuals to a simple absorbed power law in the 0.5-10 keV band remain constant with time in spite of large variations in flux. This behavior implies an unchanging source geometry and the same emission processes continuously at work at the timescale probed. With the constraints from NuSTAR on the broad-band spectral shape, it is clear that the soft excess in this source is a superposition of two different processes, one being blurred ionized reflection in the innermost parts of the accretion disk, and the other a continuum component such as a spatially distinct Comptonizing region. Alternatively, a more complex primary Comptonization component together with blurred ionized reflection could be responsible.
C1 [Lohfink, A. M.; Pinto, C.; Alston, W.; Fabian, A. C.; Kara, E.; Parker, M. L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.; Hailey, C. J.] Danish Tech Univ, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Matt, G.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Stern, D.; Walton, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
RP Lohfink, AM (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
EM alohfink@ast.cam.ac.uk
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Reynolds,
Christopher/0000-0002-1510-4860; Pinto, Ciro/0000-0003-2532-7379
FU ERC Advanced Grant FEEDBACK; Simons Foundation Fellows Program (US);
Sackler Fellowship Program (Cambridge); National Aeronautics and Space
Administration
FX We thank the referee for comments that have helped to improve the
clarity of the paper. AL and ACF acknowledge support from the ERC
Advanced Grant FEEDBACK. CSR thanks the Simons Foundation Fellows
Program (US) and the Sackler Fellowship Program (Cambridge) for support.
This work made use of data from the NuSTAR mission, a project led by the
California Institute of Technology, managed by the Jet Propulsion
Laboratory, and funded by the National Aeronautics and Space
Administration. This research has made use of the NuSTAR Data Analysis
Software (NuSTARDAS) jointly developed by the ASI Science Data Center
(ASDC, Italy) and the California Institute of Technology (USA). This
research has made use of data obtained from the Suzaku satellite, a
collaborative mission between the space agencies of Japan (JAXA) and the
USA (NASA).
NR 39
TC 4
Z9 4
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 11
DI 10.3847/0004-637X/821/1/11
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000011
ER
PT J
AU Partridge, B
Lopez-Caniego, M
Perley, RA
Stevens, J
Butler, BJ
Rocha, G
Walter, B
Zacchei, A
AF Partridge, B.
Lopez-Caniego, M.
Perley, R. A.
Stevens, J.
Butler, B. J.
Rocha, G.
Walter, B.
Zacchei, A.
TI ABSOLUTE CALIBRATION OF THE RADIO ASTRONOMY FLUX DENSITY SCALE AT 22 TO
43 GHz USING PLANCK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: interferometers; methods: observational; radio
continuum: general; techniques: interferometric; techniques: photometric
ID MICROWAVE; PLANETS; ARRAY; MAPS
AB The Planck mission detected thousands of extragalactic radio sources at frequencies from 28 to 857 GHz. Planck's calibration is absolute (in the sense that it is based on the satellite's annual motion around the Sun and the temperature of the cosmic microwave background), and its beams are well characterized at sub-percent levels. Thus, Planck's flux density measurements of compact sources are absolute in the same sense. We have made coordinated Very Large Array (VLA) and Australia Telescope Compact Array (ATCA) observations of 65 strong, unresolved Planck sources in order to transfer Planck's calibration to ground-based instruments at 22, 28, and 43 GHz. The results are compared to microwave flux density scales currently based on planetary observations. Despite the scatter introduced by the variability of many of the sources, the flux density scales are determined to 1%-2% accuracy. At 28 GHz, the flux density scale used by the VLA runs 2%-3% +/- 1.0% below Planck values with an uncertainty of +/- 1.0%; at 43 GHz, the discrepancy increases to 5%-6% +/- 1.4% for both ATCA and the VLA.
C1 [Partridge, B.; Walter, B.] Haverford Coll, Dept Astron, 370 Lancaster Ave, Haverford, PA 19041 USA.
[Lopez-Caniego, M.] European Space Agcy, ESAC, Camino Bajo Castillo S-N, Madrid, Spain.
[Lopez-Caniego, M.] Univ Cantabria, CSIC, Inst Fis Cantabria, Avda Castros S-N, E-39005 Santander, Spain.
[Perley, R. A.; Butler, B. J.] Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA.
[Stevens, J.] CSIRO, Astron & Space Sci, Paul Wild Observ, 1828 Yarrie Lake Rd, Narrabri, NSW 2390, Australia.
[Rocha, G.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA.
[Rocha, G.] CALTECH, Pasadena, CA 91125 USA.
[Zacchei, A.] INAF, Osservatorio Astron Trieste, Via GB Tiepolo 11, Trieste, Italy.
RP Partridge, B (reprint author), Haverford Coll, Dept Astron, 370 Lancaster Ave, Haverford, PA 19041 USA.
RI Lopez-Caniego, Marcos/M-4695-2013;
OI Zacchei, Andrea/0000-0003-0396-1192
FU Spanish MINECO [AYA2012-39475-C02-01, CSD2010-00064]; ESA; CNES
(France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF
(Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain);
MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland);
CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space
(Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES
(Portugal); ERC (EU); PRACE (EU)
FX We are deeply indebted to Kris Gorski, Sanjit Mitra, and Luca Pagano of
the FEBeCoP team who helped in the construction of the beams used to
derive flux densities from the Planck maps. The dates that Planck
observed each source were supplied by Jonathan Leon Tavares, then at
Aalto University, Finland. M.L.C. acknowledges the Spanish MINECO
Projects AYA2012-39475-C02-01 and Consolider-Ingenio 2010 CSD2010-00064.
The Planck Collaboration acknowledges the support of the following: ESA;
CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA
and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain);
Tekes, AoF, and CSC (Finland); DLR and MPG(Germany); CSA (Canada); DTU
Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland);
FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck
Collaboration and a list of its members, indicating which technical or
scientific activities they have been involved in, can be found at
http://www.cosmos.esa.int/web/planck.
NR 39
TC 3
Z9 3
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 61
DI 10.3847/0004-637X/821/1/61
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000061
ER
PT J
AU Preece, R
Goldstein, A
Bhat, N
Stanbro, M
Hakkila, J
Blalock, D
AF Preece, Robert
Goldstein, Adam
Bhat, Narayana
Stanbro, Matthew
Hakkila, Jon
Blalock, Dylan
TI WHICH E-peak? THE CHARACTERISTIC ENERGY OF GAMMA-RAY BURST SPECTRA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; methods: data analysis
ID BATSE OBSERVATIONS; GRB 130427A; PULSE; LONG; EVOLUTION; BRIGHT;
CATALOG; LUMINOSITY; SIGNATURES; LAG
AB A characteristic energy of individual gamma-ray burst (GRB) spectra can in most cases be determined from the peak energy of the energy density spectra (F-nu(nu)), called "E-peak." Distributions of E-peak have been compiled for time-resolved spectra from bright GRBs, as well as. time-averaged spectra and peak. flux spectra for nearly every burst observed by the Compton Gamma. Ray. Observatory. Burst And Transient Source Experiment and the Fermi. Gamma-ray Burst Monitor (GBM). Even when determined by an instrument with a broad energy band, such as GBM (8 keV to 40MeV), the distributions themselves peak at around 240 keV in the observer's frame, with a spread of roughly a decade in energy. E-peak can have considerable evolution (sometimes greater than one decade) within any given burst, as amply demonstrated by single pulses in GRB. 110721A and GRB. 130427A. Meanwhile, several luminosity or energy relations have been proposed to correlate with either the timeintegrated or peak. flux E-peak. Thus, when discussing correlations with E-peak, the question arises, "Which E-peak?". A single burst may be characterized by any. of a number of values for E-peak that are associated with it. Using a single-pulse simulation model with spectral evolution as a proxy for the type of spectral evolution observed in many bursts, we investigate how the time-averaged E-peak emerges from the spectral evolution within a single pulse, how this average naturally correlates with the peak. flux. derived Epeak in a burst, and how the distribution in E-peak values from many bursts derives its surprisingly narrow width.
C1 [Preece, Robert] Univ Alabama, Dept Space Sci, Huntsville, AL 35809 USA.
[Goldstein, Adam] NASA, Space Sci Off, Marshall Space Flight Ctr, VP62, Huntsville, AL 35812 USA.
[Bhat, Narayana; Stanbro, Matthew] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35809 USA.
[Hakkila, Jon] Univ Charleston, SC Coll Charleston, Charleston, SC 29424 USA.
[Blalock, Dylan] Univ Alabama, Dept Phys, Huntsville, AL 35809 USA.
RP Preece, R (reprint author), Univ Alabama, Dept Space Sci, Huntsville, AL 35809 USA.
EM rob.preece@nasa.gov
OI Preece, Robert/0000-0003-1626-7335
NR 43
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 12
DI 10.3847/0004-637X/821/1/12
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000012
ER
PT J
AU Taquet, V
Wirstrom, ES
Charnley, SB
AF Taquet, Vianney
Wirstrom, Eva S.
Charnley, Steven B.
TI FORMATION AND RECONDENSATION OF COMPLEX ORGANIC MOLECULES DURING
PROTOSTELLAR LUMINOSITY OUTBURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: abundances; ISM: molecules; stars: formation
ID YOUNG STELLAR OBJECTS; SPITZER SPECTROSCOPIC SURVEY;
GRAIN-SURFACE-CHEMISTRY; MASSIVE STAR-FORMATION; GAS-PHASE FORMATION;
INTERSTELLAR-MEDIUM; METHYL FORMATE; HOT AMMONIA; DISSOCIATIVE
RECOMBINATION; THERMAL-DESORPTION
AB During the formation of stars, the accretion of surrounding material toward the central object is thought to undergo strong luminosity outbursts followed by long periods of relative quiescence, even at the early stages of star formation when the protostar is still embedded in a large envelope. We investigated the gas-phase formation and recondensation of the complex organic molecules (COMs) di-methyl ether and methyl formate, induced by sudden ice evaporation processes occurring during luminosity outbursts of different amplitudes in protostellar envelopes. For this purpose, we updated a gas-phase chemical network forming COMs in which ammonia plays a key role. The model calculations presented here demonstrate that ion-molecule reactions alone could account for the observed presence of di-methyl ether and methyl formate in a large fraction of protostellar cores without recourse to grain-surface chemistry, although they depend on uncertain ice abundances and gas-phase reaction branching ratios. In spite of the short outburst timescales of about 100 years, abundance ratios of the considered species higher than 10% with respect to methanol are predicted during outbursts due to their low binding energies relative to water and methanol which delay their recondensation during cooling. Although the current luminosity of most embedded protostars would be too low to produce complex organics in the hot-core regions that are observable with current sub-millimetric interferometers, previous luminosity outburst events would induce the formation of COMs in extended regions of protostellar envelopes with sizes increasing by up to one order of magnitude.
C1 [Taquet, Vianney] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Wirstrom, Eva S.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
[Charnley, Steven B.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Charnley, Steven B.] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Taquet, V (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
OI Wirstrom, Eva/0000-0002-0656-876X
FU European Union A-ERC grant [291141 CHEMPLAN]; NASA postdoctoral program;
Swedish National Space Board; NASA's Origins of Solar Systems Program
FX We thank the anonymous referee for insightful comments that helped to
improve the quality of the manuscript. This work is supported by the
European Union A-ERC grant 291141 CHEMPLAN. V.T. acknowledges the
support from the NASA postdoctoral program. E.S.W. acknowledges generous
financial support from the Swedish National Space Board. S.B.C. was
supported by NASA's Origins of Solar Systems Program.
NR 82
TC 3
Z9 3
U1 3
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2016
VL 821
IS 1
AR 46
DI 10.3847/0004-637X/821/1/46
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9GB
UT WOS:000373809000046
ER
PT J
AU Carrasco-Gonzalez, C
Henning, T
Chandler, CJ
Linz, H
Perez, L
Rodriguez, LF
Galvan-Madrid, R
Anglada, G
Birnstiel, T
van Boekel, R
Flock, M
Klahr, H
Macias, E
Menten, K
Osorio, M
Testi, L
Torrelles, JM
Zhu, ZH
AF Carrasco-Gonzalez, Carlos
Henning, Thomas
Chandler, Claire J.
Linz, Hendrik
Perez, Laura
Rodriguez, Luis F.
Galvan-Madrid, Roberto
Anglada, Guillem
Birnstiel, Til
van Boekel, Roy
Flock, Mario
Klahr, Hubert
Macias, Enrique
Menten, Karl
Osorio, Mayra
Testi, Leonardo
Torrelles, Jose M.
Zhu, Zhaohuan
TI THE VLA VIEW OF THE HL TAU DISK: DISK MASS, GRAIN EVOLUTION, AND EARLY
PLANET FORMATION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: formation; protoplanetary disks; stars:
formation; stars: individual (HL Tau); stars: protostars; techniques:
interferometric
ID CIRCUMSTELLAR DISK; PROTOPLANETARY DISKS; DUST EMISSION; HL/XZ-TAU;
GROWTH; REGION; GAPS; BINARY; JET
AB The first long-baseline ALMA campaign resolved the disk around the young star HL Tau into a number of axisymmetric bright and dark rings. Despite the very young age of HL Tau, these structures have been interpreted as signatures for the presence of (proto) planets. The ALMA images triggered numerous theoretical studies based on disk-planet interactions, magnetically driven disk structures, and grain evolution. Of special interest are the inner parts of disks, where terrestrial planets are expected to form. However, the emission from these regions in HL. Tau turned out to be optically thick at all ALMA wavelengths, preventing the derivation of surface density profiles and grain-size distributions. Here, we present the most sensitive images of HL. Tau obtained to date with the Karl G. Jansky Very Large Array at 7.0 mm wavelength with a spatial resolution comparable to the ALMA images. At this long wavelength, the dust emission from HL Tau is optically thin, allowing a comprehensive study of the inner disk. We obtain a total disk dust mass of (1-3) x 10(-3) M-circle dot, depending on the assumed opacity and disk temperature. Our optically thin data also indicate fast grain growth, fragmentation, and formation of dense clumps in the inner densest parts of the disk. Our results suggest that the HL. Tau disk may be actually in a very early stage of planetary formation, with planets not already formed in the gaps but in the process of future formation in the bright rings.
C1 [Carrasco-Gonzalez, Carlos; Rodriguez, Luis F.; Galvan-Madrid, Roberto] UNAM, Inst Radioastron & Astrofis, Apartado Postal 3-72 Xangari, Morelia 58089, Michoacan, Mexico.
[Henning, Thomas; Linz, Hendrik; Birnstiel, Til; van Boekel, Roy; Klahr, Hubert] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Chandler, Claire J.; Perez, Laura; Menten, Karl] Natl Radio Astron Observ, POB O,1003 Lopezville Rd, Socorro, NM 87801 USA.
[Perez, Laura] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Anglada, Guillem; Macias, Enrique; Osorio, Mayra] CSIC, Inst Astrofis Andalucia, Apartado 3004, E-18080 Granada, Spain.
[Flock, Mario] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Testi, Leonardo] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Testi, Leonardo] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy.
[Testi, Leonardo] Excellence Cluster Universe, Boltzmann Str 2, D-85748 Garching, Germany.
[Torrelles, Jose M.] CSIC, Inst Ciencies Espai, IEEC, Marti & Franques 1, E-08028 Barcelona, Spain.
[Torrelles, Jose M.] UB, Inst Ciencies Cosmos, IEEC, Marti & Franques 1, E-08028 Barcelona, Spain.
[Zhu, Zhaohuan] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Carrasco-Gonzalez, C; Rodriguez, LF; Galvan-Madrid, R (reprint author), UNAM, Inst Radioastron & Astrofis, Apartado Postal 3-72 Xangari, Morelia 58089, Michoacan, Mexico.; Henning, T; Linz, H; Birnstiel, T; van Boekel, R; Klahr, H (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.; Chandler, CJ; Perez, L; Menten, K (reprint author), Natl Radio Astron Observ, POB O,1003 Lopezville Rd, Socorro, NM 87801 USA.; Perez, L (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.; Anglada, G; Macias, E; Osorio, M (reprint author), CSIC, Inst Astrofis Andalucia, Apartado 3004, E-18080 Granada, Spain.; Flock, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Testi, L (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.; Testi, L (reprint author), INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy.; Testi, L (reprint author), Excellence Cluster Universe, Boltzmann Str 2, D-85748 Garching, Germany.
EM c.carrasco@crya.unam.mx; henning@mpia.de; cchandle@nrao.edu;
linz@mpia.de; lperez@mpifr.de; l.rodriguez@crya.unam.mx;
r.galvan@crya.unam.mx; guillem@iaa.es; birnstiel@mpia.de;
boekel@mpia.de; mario.flock@jpl.nasa.gov; klahr@mpia.de; emacias@iaa.es;
kmenten@mpifr.de; osorio@iaa.es; ltesti@eso.org
OI Macias, Enrique/0000-0003-1283-6262; Torrelles, Jose
Maria/0000-0002-6896-6085; Birnstiel, Tilman/0000-0002-1899-8783
FU UNAM-DGAPA PAPIIT [IA101715, IA102816]; Alexander van Humboldt
Foundation; DFG [KL 1469/13-1]; MINECO; FEDER funds
FX C.C.-G., L.F.R., and R.G.-M. acknowledge support from UNAM-DGAPA PAPIIT
IA101715 and IA102816. L.M.P. acknowledges support from the Alexander
van Humboldt Foundation. T.B. acknowledges support from the DFG grant
(KL 1469/13-1). G.A., E.M., M.O., and J.M.T. acknowledge support from
MINECO and FEDER funds. ALMA is a partnership of ESO (representing its
member states), NSF (USA) and NINS (Japan), together with NRC (Canada),
NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation
with the Republic of Chile. The Joint ALMA Observatory is operated by
ESO, AUI/NRAO and NAOJ.
NR 34
TC 6
Z9 6
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2016
VL 821
IS 1
AR L16
DI 10.3847/2041-8205/821/1/L16
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9HA
UT WOS:000373812000016
ER
PT J
AU Kim, JW
Im, M
Lee, SK
Edge, AC
Hyun, M
Kim, D
Choi, C
Hong, J
Jeon, Y
Jun, HD
Karouzos, M
Kim, D
Kim, JH
Kim, Y
Park, WK
Taak, YC
Yoon, Y
AF Kim, Jae-Woo
Im, Myungshin
Lee, Seong-Kook
Edge, Alastair C.
Hyun, Minhee
Kim, Dohyeong
Choi, Changsu
Hong, Jueun
Jeon, Yiseul
Jun, Hyunsung David
Karouzos, Marios
Kim, Duho
Kim, Ji Hoon
Kim, Yongjung
Park, Won-Kee
Taak, Yoon Chan
Yoon, Yongmin
TI DISCOVERY OF A SUPERCLUSTER AT z similar to 0.91 AND TESTING THE Lambda
CDM COSMOLOGICAL MODEL
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: clusters: general; galaxies: high-redshift
ID DEEP EXTRAGALACTIC SURVEY; GALAXY CLUSTER; STAR-FORMATION; VORONOI
TESSELLATION; RED GALAXIES; EVOLUTION; UKIDSS; SCALE; COLOR; DIMENSIONS
AB The Lambda CDM cosmological model successfully reproduces many aspects of the galaxy and structure formation of the universe. However, the growth of large-scale structures (LSSs) in the early universe is not well tested yet with observational data. Here, we have utilized wide and deep optical-near-infrared data in order to search for distant galaxy clusters and superclusters (0.8 < z < 1.2). From the spectroscopic observation with the Inamori Magellan Areal Camera and Spectrograph (IMACS) on the Magellan telescope, three massive clusters at z similar to 0.91 are confirmed in the SSA22 field. Interestingly, all of them have similar redshifts within Delta z similar to 0.01 with velocity dispersions ranging from 470 to 1300 km s(-1). Moreover, as the maximum separation is similar to 15 Mpc, they compose a supercluster at z similar to 0.91, meaning that this is one of the most massive superclusters at this redshift to date. The galaxy density map implies that the confirmed clusters are embedded in a larger structure stretching over similar to 100 Mpc. Lambda CDM models predict about one supercluster like this in our surveyed volume, consistent with our finding so far. However, there are more supercluster candidates in this field, suggesting that additional studies are required to determine if the Lambda CDM cosmological model can successfully reproduce the LSSs at high redshift.
C1 [Kim, Jae-Woo; Im, Myungshin; Lee, Seong-Kook; Hyun, Minhee; Kim, Dohyeong; Choi, Changsu; Hong, Jueun; Kim, Yongjung; Taak, Yoon Chan; Yoon, Yongmin] Seoul Natl Univ, Dept Phys & Astron, Ctr Explorat Origin Universe, Seoul 151742, South Korea.
[Kim, Jae-Woo; Im, Myungshin; Lee, Seong-Kook; Hyun, Minhee; Kim, Dohyeong; Choi, Changsu; Hong, Jueun; Jeon, Yiseul; Jun, Hyunsung David; Karouzos, Marios; Kim, Duho; Kim, Yongjung; Taak, Yoon Chan; Yoon, Yongmin] Seoul Natl Univ, Dept Phys & Astron, Astron Program, FPRD, Seoul 151742, South Korea.
[Edge, Alastair C.] Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England.
[Jun, Hyunsung David] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Kim, Duho] Arizona State Univ, Sch Earth & Space Explorat, POB 871404, Tempe, AZ 85287 USA.
[Kim, Ji Hoon] Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA.
[Park, Won-Kee] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea.
RP Kim, JW; Im, M (reprint author), Seoul Natl Univ, Dept Phys & Astron, Ctr Explorat Origin Universe, Seoul 151742, South Korea.; Kim, JW; Im, M (reprint author), Seoul Natl Univ, Dept Phys & Astron, Astron Program, FPRD, Seoul 151742, South Korea.
EM kjw0704@gmail.com; mim@astro.snu.ac.kr
FU National Research Foundation of Korea (NRF) - Korea government (MSIP)
[2008-0060544]; STFC grant [ST/L00075X/1]; NRF-Fostering Core Leaders of
Future Program - Korean government [2015000714]; Global PH.D Fellowship
Program through the National Research Foundation of Korea (NRF) -
Ministry of Education [NRF-2013H1A2A1033110]; ESO Very Large Telescope,
under the "Large Programme" [182.A-0886]
FX Authors thank an anonymous referee for comments that were useful for
improving the paper. This work was supported by the National Research
Foundation of Korea (NRF) grant, No. 2008-0060544, funded by the Korea
government (MSIP). A.C.E. acknowledges support from STFC grant
ST/L00075X/1. D.K. acknowledges fellowship support from the grant
NRF-2015-Fostering Core Leaders of Future Program, No. 2015000714,
funded by the Korean government. M.H. acknowledges the support from
Global PH.D Fellowship Program through the National Research Foundation
of Korea (NRF) funded by the Ministry of Education
(NRF-2013H1A2A1033110). We are grateful to UKIDSS team, the staff in
UKIRT, Cambridge Astronomical Survey Unit and Wide Field Astronomy Unit
in Edinburgh. The United Kingdom Infrared Telescope was run by the Joint
Astronomy Centre on behalf of the Science and Technology Facilities
Council of the U.K. This work is based in part on data products produced
at the Canadian Astronomy Data Centre as part of the
Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of
NRC and CNRS. This Letter uses data from the VIMOS Public Extragalactic
Redshift Survey (VIPERS). VIPERS has been performed using the ESO Very
Large Telescope, under the "Large Programme" 182.A-0886. The
participating institutions and funding agencies are listed at
http://vipers.inaf.it. This research uses data from the VIMOS VLT Deep
Survey, obtained from the VVDS database operated by Cesam, Laboratoire
d'Astrophysique de Marseille, France. Finally, authors also thank staff
in the Las Campanas Observatory.
NR 38
TC 1
Z9 1
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2016
VL 821
IS 1
AR L10
DI 10.3847/2041-8205/821/1/L10
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9HA
UT WOS:000373812000010
ER
PT J
AU Kitiashvili, IN
Kosovichev, AG
Mansour, NN
Wray, AA
AF Kitiashvili, I. N.
Kosovichev, A. G.
Mansour, N. N.
Wray, A. A.
TI DYNAMICS OF TURBULENT CONVECTION AND CONVECTIVE OVERSHOOT IN A
MODERATE-MASS STAR
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE asteroseismology; convection; methods: numerical; stars: general; stars:
interiors; Sun: helioseismology
ID STELLAR EVOLUTION CALCULATIONS; COMPRESSIBLE CONVECTION; NUMERICAL
SIMULATIONS; RADIAL OSCILLATIONS; SOLAR OSCILLATIONS; MODELS; SUN;
HELIOSEISMOLOGY; PENETRATION; EXCITATION
AB We present results of realistic three-dimensional (3D) radiative hydrodynamic simulations of the outer layers of a moderate-mass star (1.47 M-circle dot), including the full convection zone, the overshoot region, and the top layers of the radiative zone. The simulation results show that the surface granulation has a broad range of scales, from 2 to 12 Mm, and that large granules are organized in well-defined clusters, consisting of several granules. Comparison of the mean structure profiles from 3D simulations with the corresponding one-dimensional (1D) standard stellar model shows an increase of the stellar radius by similar to 800 km, as well as significant changes in the thermodynamic structure and turbulent properties of the ionization zones. Convective downdrafts in the intergranular lanes between granulation clusters reach speeds of more than 20 km s(-1), penetrate through the whole convection zone, hit the radiative zone, and form an 8Mm thick overshoot layer. Contrary to semi-empirical overshooting models, our results show that the 3D dynamic overshoot region consists of two layers: a nearly adiabatic extension of the convection zone and a deeper layer of enhanced subadiabatic stratification. This layer is formed because of heating caused by the braking of the overshooting convective plumes. This effect has to be taken into account in stellar modeling and the interpretation of asteroseismology data. In particular, we demonstrate that the deviations of the mean structure of the 3D model from the 1D standard model of the same mass and composition are qualitatively similar to the deviations for the Sun found by helioseismology.
C1 [Kitiashvili, I. N.; Mansour, N. N.; Wray, A. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kosovichev, A. G.] New Jersey Inst Technol, Newark, NJ 07102 USA.
RP Kitiashvili, IN (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM irina.n.kitiashvili@nasa.gov
OI Kitiashvili, Irina/0000-0003-4144-2270
NR 36
TC 2
Z9 2
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2016
VL 821
IS 1
AR L17
DI 10.3847/2041-8205/821/1/L17
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9HA
UT WOS:000373812000017
ER
PT J
AU Kospal, A
Abraham, P
Csengeri, T
Gorti, U
Henning, T
Moor, A
Semenov, DA
Szucs, L
Gusten, R
AF Kospal, A.
Abraham, P.
Csengeri, T.
Gorti, U.
Henning, Th.
Moor, A.
Semenov, D. A.
Szucs, L.
Guesten, R.
TI COLD CO GAS IN THE DISK OF THE YOUNG ERUPTIVE STAR EX LUP
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE stars: individual(EX Lup); stars: pre-main sequence; stars: variables: T
Tauri, Herbig Ae/Be
ID 2008 EXTREME OUTBURST; T-TAURI-STARS; CIRCUMSTELLAR DISKS; ACCRETION;
BINARIES; SPECTROSCOPY; TRANSITION; EMISSION
AB EX. Lupi-type objects (EXors) form a sub-class of T Tauri stars, defined by sudden sporadic flare-ups of 1-5 mag at optical wavelengths. These eruptions are attributed to enhanced mass accretion from the circumstellar disk to the star, and may constitute important events in shaping the structure of the inner disk and the forming planetary system. Although disk properties must play a fundamental role in driving the outbursts, they are surprisingly poorly known. In order to characterize the dust and gas components of EXor disks, here we report on observations of the (CO)-C-12 J = 3-2 and 4-3 lines, and the (CO)-C-13 3-2 line in EX Lup, the prototype of the EXor class. We reproduce the observed line fluxes and profiles with a line radiative transfer model and compare the obtained parameters with corresponding ones of other T Tauri disks.
C1 [Kospal, A.; Abraham, P.; Moor, A.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, POB 67, H-1525 Budapest, Hungary.
[Kospal, A.; Henning, Th.; Semenov, D. A.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Csengeri, T.; Guesten, R.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Gorti, U.] SETI Inst, Mountain View, CA USA.
[Gorti, U.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Szucs, L.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
RP Kospal, A (reprint author), Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, POB 67, H-1525 Budapest, Hungary.; Kospal, A (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM kospal@konkoly.hu
RI Semenov, Dmitry/B-7446-2012;
OI Semenov, Dmitry/0000-0002-3913-7114; Szucs, Laszlo/0000-0002-6771-1689
FU Momentum grant of the MTA CSFK Lendluet Disk Research Group; Hungarian
Research Fund OTKA grant [K101393]; Bolyai Research Fellowship of the
Hungarian Academy of Sciences
FX This work was supported by the Momentum grant of the MTA CSFK Lendluet
Disk Research Group, and the Hungarian Research Fund OTKA grant K101393.
A.M. acknowledges support from the Bolyai Research Fellowship of the
Hungarian Academy of Sciences.
NR 31
TC 2
Z9 2
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2016
VL 821
IS 1
AR L4
DI 10.3847/2041-8205/821/1/L4
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9HA
UT WOS:000373812000004
ER
PT J
AU Miller, JM
Raymond, J
Fabian, AC
Gallo, E
Kaastra, J
Kallman, T
King, AL
Proga, D
Reynolds, CS
Zoghbi, A
AF Miller, J. M.
Raymond, J.
Fabian, A. C.
Gallo, E.
Kaastra, J.
Kallman, T.
King, A. L.
Proga, D.
Reynolds, C. S.
Zoghbi, A.
TI THE ACCRETION DISK WIND IN THE BLACK HOLE GRS 1915+105
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; black hole physics; X-rays: binaries
ID X-RAY BINARIES; INNER DISK; MASS; SPIN; OUTFLOWS; CORONAE; JETS; GAS;
SPECTROSCOPY; SIMULATIONS
AB We report on a 120 ks Chandra/HETG spectrum of the black hole GRS 1915+105. The observation was made during an extended and bright soft state in 2015 June. An extremely rich disk wind absorption spectrum is detected, similar to that observed at lower sensitivity in 2007. The very high resolution of the third-order spectrum reveals four components to the disk wind in the Fe K band alone; the fastest has a blueshift of v = 0.03c. Broadened re-emission from the wind is also detected in the first-order spectrum, giving rise to clear accretion disk P Cygni profiles. Dynamical modeling of the re-emission spectrum gives wind launching radii of r similar or equal to 10(2-4) GM/c(2). Wind density values of n similar or equal to 10(13-16) cm(-3) are then required by the ionization parameter formalism. The small launching radii, high density values, and inferred high mass outflow rates signal a role for magnetic driving. With simple, reasonable assumptions, the wind properties constrain the magnitude of the emergent magnetic field to be B similar or equal to 10(3-4) G if the wind is driven via magnetohydrodynamic (MHD) pressure from within the disk. and B similar or equal to 10(4-5) G if the wind is driven by magnetocentrifugal acceleration. The MHD estimates are below upper limits predicted by the canonical alpha-disk model. We discuss these results in terms of fundamental disk physics and black hole accretion modes.
C1 [Miller, J. M.; Gallo, E.; Zoghbi, A.] Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48109 USA.
[Raymond, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 OHA, England.
[Kaastra, J.] SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
[Kaastra, J.] Univ Utrecht, Dept Phys & Astron, POB 80000, NL-3508 TA Utrecht, Netherlands.
[Kallman, T.] NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
[King, A. L.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA.
[Proga, D.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA.
[Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48109 USA.
EM jonmm@umich.edu
RI Zoghbi, Abderahmen/A-8445-2017
OI Zoghbi, Abderahmen/0000-0002-0572-9613
NR 41
TC 4
Z9 4
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2016
VL 821
IS 1
AR L9
DI 10.3847/2041-8205/821/1/L9
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9HA
UT WOS:000373812000009
ER
PT J
AU Parker, ML
Tomsick, JA
Kennea, JA
Miller, JM
Harrison, FA
Barret, D
Boggs, SE
Christensen, FE
Craig, WW
Fabian, AC
Furst, F
Grinberg, V
Hailey, CJ
Romano, P
Stern, D
Walton, DJ
Zhang, WW
AF Parker, M. L.
Tomsick, J. A.
Kennea, J. A.
Miller, J. M.
Harrison, F. A.
Barret, D.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Fabian, A. C.
Fuerst, F.
Grinberg, V.
Hailey, C. J.
Romano, P.
Stern, D.
Walton, D. J.
Zhang, W. W.
TI NuSTAR AND SWIFT OBSERVATIONS OF THE VERY HIGH STATE IN GX 339-4:
WEIGHING THE BLACK HOLE WITH X-RAYS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; X-rays: binaries; X-rays: individual (GX
339-4)
ID CYGNUS X-1; COMPTONIZATION MODELS; ACCRETION DISK; HARD STATE; SPIN;
SPECTROSCOPY; REFLECTION; GX-339-4; BINARIES; SUZAKU
AB We present results from spectral fitting of the very high state of GX 339-4 with Nuclear Spectroscopic Telescope Array (NuSTAR) and Swift. We use relativistic reflection modeling to measure the spin of the black hole and inclination of the inner disk and find a spin of a = 0.95(-0.08)(+0.02) and inclination of 30 degrees +/- 1 degrees (statistical errors). These values agree well with previous results from reflection modeling. With the exceptional sensitivity of NuSTAR at the high-energy side of the disk spectrum, we are able to constrain multiple physical parameters simultaneously using continuum fitting. By using the constraints from reflection as input for the continuum fitting method, we invert the conventional fitting procedure to estimate the mass and distance of GX 339-4 using just the X-ray spectrum, finding a mass of 9.0(-1.2)(+1.6) M-circle dot and distance of 8.4 +/- 0.9 kpc (statistical errors).
C1 [Parker, M. L.; Fabian, A. C.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Tomsick, J. A.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
[Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Miller, J. M.] Univ Michigan, Dept Astron, 1085 South Univ Ave,West Hall 311, Ann Arbor, MI 48109 USA.
[Harrison, F. A.; Fuerst, F.] CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
[Barret, D.] Inst Rech Astrophys & Planetol, 9 Ave Colonel Roche, F-31028 Toulouse, France.
[Christensen, F. E.] Danish Tech Univ, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Grinberg, V.] MIT, Kavli Inst Astrophys, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Hailey, C. J.] Columbia Univ, New York, NY 10027 USA.
[Romano, P.] INAF IASF Palermo, Via Ugo La Malfa 153, I-90146 Palermo, Italy.
[Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Parker, ML (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Parker, Michael/0000-0002-8466-7317
FU STFC; NASA; [ASI-INAF I/004/11/0]; [ASI-INAF I/037/12/0]
FX We are grateful to the referee for detailed and thoughtful comments that
have significantly improved the paper. M.L.P. acknowledges financial
support from the STFC. P.R. acknowledges financial contribution from
ASI-INAF I/004/11/0 and ASI-INAF I/037/12/0. This work made use of data
from the NuSTAR mission, a project led by the California Institute of
Technology, managed by the Jet Propulsion Laboratory, and funded by
NASA. This research has made use of the NuSTAR Data Analysis Software
(NuSTARDAS) jointly developed by the ASI Science Data Center and the
California Institute of Technology.
NR 40
TC 5
Z9 5
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2016
VL 821
IS 1
AR L6
DI 10.3847/2041-8205/821/1/L6
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9HA
UT WOS:000373812000006
ER
PT J
AU Serigano, J
Nixon, CA
Cordiner, MA
Irwin, PGJ
Teanby, NA
Charnley, SB
Lindberg, JE
AF Serigano, Joseph
Nixon, C. A.
Cordiner, M. A.
Irwin, P. G. J.
Teanby, N. A.
Charnley, S. B.
Lindberg, J. E.
TI ISOTOPIC RATIOS OF CARBON AND OXYGEN IN TITAN'S CO USING ALMA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: individual
(Titan); techniques: imaging spectroscopy; techniques: interferometric
ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; FAR-INFRARED SPECTRA;
VERTICAL-DISTRIBUTION; ATMOSPHERE; PAIRS; TEMPERATURES; 300-K;
STRATOSPHERE; ABUNDANCES; DISCOVERY
AB We report interferometric observations of carbon monoxide (CO) and its isotopologues in Titan's atmosphere using the Atacama Large Millimeter/submillimeter Array (ALMA). The following transitions were detected: CO (J = 1-0, 2-1, 3-2, 6-5), (CO)-C-13 (J = 2-1, 3-2, 6-5), (CO)-O-18 (J = 2-1, 3-2), and (CO)-O-17 (J = 3-2). Molecular abundances and the vertical atmospheric temperature profile were derived by modeling the observed emission line profiles using NEMESIS, a line-by-line radiative transfer code. We present the first spectroscopic detection of O-17 in the outer solar system with (CO)-O-17 detected at >8 sigma confidence. The abundance of CO was determined to be 49.6 +/- 1.8 ppm, assumed to be constant with altitude, with isotopic ratios C-12/C-13 = 89.9 +/- 3.4, O-16/O-18 = 486 +/- 22, and O-16/O-17 = 2917 +/- 359. The measurements of C-12/C-13 and O-16/O-18 ratios are the most precise values obtained in Titan's atmospheric CO to date. Our results are in good agreement with previous studies and suggest no significant deviations from standard terrestrial isotopic ratios.
C1 [Serigano, Joseph; Nixon, C. A.; Cordiner, M. A.; Charnley, S. B.; Lindberg, J. E.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Serigano, Joseph; Cordiner, M. A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Irwin, P. G. J.] Univ Oxford, Clarendon Lab, Atmospher Ocean & Planetary Phys, Parks Rd, Oxford OX1 3PU, England.
[Teanby, N. A.] Univ Bristol, Sch Earth Sci, Wills Mem Bldg,Queens Rd, Bristol BS8 1RJ, Avon, England.
[Serigano, Joseph] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
RP Serigano, J (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.; Serigano, J (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.; Serigano, J (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
EM jserigano4@jhu.edu
RI Nixon, Conor/A-8531-2009;
OI Nixon, Conor/0000-0001-9540-9121; Teanby, Nicholas/0000-0003-3108-5775;
Irwin, Patrick/0000-0002-6772-384X
FU UK Science and Technology Facilities Council
FX We would like to acknowledge the staff at the helpdesk of the North
American ALMA Science Center (NAASC) in Charlottesville, Virginia, for
providing helpful information on the calibration of ALMA data. N.A.T.
and P.G.J.I. are funded by the UK Science and Technology Facilities
Council. J.E.L. is supported by an appointment to the NASA Postdoctoral
Program at the NASA Goddard Space Flight Center, administered by Oak
Ridge Associated Universities through a contract with NASA. This work
makes use of the ADS/JAO. ALMA project codes listed in Table 2. ALMA is
a partnership of ESO (representing its member states), NSF (USA) and
NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and
KASI (Republic of Korea), in cooperation with the Republic of Chile. The
Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The
National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc.
NR 33
TC 1
Z9 1
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2016
VL 821
IS 1
AR L8
DI 10.3847/2041-8205/821/1/L8
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI9HA
UT WOS:000373812000008
ER
PT J
AU Tahimic, CGT
Long, RK
Kubota, T
Sun, MY
Elalieh, H
Fong, C
Menendez, AT
Wang, YM
Vilardaga, JP
Bikle, DD
AF Tahimic, Candice G. T.
Long, Roger K.
Kubota, Takuo
Sun, Maggie Yige
Elalieh, Hashem
Fong, Chak
Menendez, Alicia T.
Wang, Yongmei
Vilardaga, Jean-Pierre
Bikle, Daniel D.
TI Regulation of Ligand and Shear Stress-induced Insulin-like Growth Factor
1 (IGF1) Signaling by the Integrin Pathway
SO JOURNAL OF BIOLOGICAL CHEMISTRY
LA English
DT Article
DE insulin-like growth factor (IGF); integrin; mechanotransduction;
osteoblast; shear stress; IGF1 receptor; IGF1 signaling
ID FOCAL ADHESION KINASE; FACTOR-I RECEPTOR; BONE-FORMATION; BED REST;
CELLS; OSTEOBLAST; ACTIVATION; OSTEOCYTES; RESISTANCE;
MECHANOTRANSDUCTION
AB Mechanical loading of the skeleton, as achieved during daily movement and exercise, preserves bone mass and stimulates bone formation, whereas skeletal unloading from prolonged immobilization leads to bone loss. A functional interplay between the insulin-like growth factor 1 receptor (IGF1R), a major player in skeletal development, and integrins, mechanosensors, is thought to regulate the anabolic response of osteogenic cells to mechanical load. The mechanistic basis for this cross-talk is unclear. Here we report that integrin signaling regulates activation of IGF1R and downstream targets in response to both IGF1 and a mechanical stimulus. In addition, integrins potentiate responsiveness of IGF1R to IGF1 and mechanical forces. We demonstrate that integrin-associated kinases, Rous sarcoma oncogene (SRC) and focal adhesion kinase (FAK), display distinct actions on IGF1 signaling; FAK regulates IGF1R activation and its downstream effectors, AKT and ERK, whereas SRC controls signaling downstream of IGF1R. These findings linked to our observation that IGF1 assembles the formation of a heterocomplex between IGF1R and integrin 3 subunit indicate that the regulation of IGF1 signaling by integrins proceeds by direct receptor-receptor interaction as a possible means to translate biomechanical forces into osteoanabolic signals.
C1 [Tahimic, Candice G. T.; Sun, Maggie Yige; Elalieh, Hashem; Fong, Chak; Menendez, Alicia T.; Wang, Yongmei; Bikle, Daniel D.] Vet Affairs Med Ctr, Endocrine Res Unit, San Francisco, CA 94121 USA.
[Tahimic, Candice G. T.; Sun, Maggie Yige; Elalieh, Hashem; Fong, Chak; Menendez, Alicia T.; Wang, Yongmei; Bikle, Daniel D.] Univ Calif San Francisco, San Francisco, CA 94158 USA.
[Long, Roger K.] Univ Calif San Francisco, Dept Pediat, San Francisco, CA 94143 USA.
[Kubota, Takuo] Osaka Univ, Dept Pediat, Osaka 5650871, Japan.
[Vilardaga, Jean-Pierre] Univ Pittsburgh, Sch Med, Dept Pharmacol & Chem Biol, Lab GPCR Biol, Pittsburgh, PA 15213 USA.
[Tahimic, Candice G. T.] NASA, Space Biosci Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bikle, DD (reprint author), 1700 Owens St,MB360, San Francisco, CA 94158 USA.
EM Daniel.Bikle@ucsf.edu
FU National Institutes of Health (NIAMS) [RO1 AR055924]; National
Institutes of Health (NIDKK) [R01 DK087688, R01DK102495]; National Space
Biomedical Research Institute [NASA NCC 9-58]
FX This work was supported, in whole or in part, by National Institutes of
Health Grants (RO1 AR055924; NIAMS, to D. D. B.) and R01 DK087688 and
R01DK102495; NIDKK, to J. P.-V.).; Supported by postdoctoral fellowship
awards from the National Space Biomedical Research Institute (NASA NCC
9-58).
NR 41
TC 2
Z9 2
U1 2
U2 9
PU AMER SOC BIOCHEMISTRY MOLECULAR BIOLOGY INC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3996 USA
SN 0021-9258
EI 1083-351X
J9 J BIOL CHEM
JI J. Biol. Chem.
PD APR 8
PY 2016
VL 291
IS 15
BP 8140
EP 8149
DI 10.1074/jbc.M115.693598
PG 10
WC Biochemistry & Molecular Biology
SC Biochemistry & Molecular Biology
GA DJ2SZ
UT WOS:000374056700031
PM 26865633
ER
PT J
AU Ackermann, M
Ajello, M
Albert, A
Atwood, WB
Baldini, L
Barbiellini, G
Bastieri, D
Bellazzini, R
Bissaldi, E
Blandford, RD
Bonino, R
Bottacini, E
Bregeon, J
Bruel, P
Buehler, R
Caliandro, GA
Cameron, RA
Caragiulo, M
Caraveo, PA
Cavazzuti, E
Cecchi, C
Chekhtman, A
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Costanza, F
Cuoco, A
Cutini, S
D'Ammando, F
de Angelis, A
de Palma, F
Desiante, R
Digel, SW
Di Venere, L
Drell, PS
Favuzzi, C
Fegan, SJ
Focke, WB
Franckowiak, A
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grove, JE
Guiriec, S
Harding, AK
Hewitt, JW
Horan, D
Hou, X
Iafrate, G
Johannesson, G
Kamae, T
Kuss, M
Larsson, S
Latronico, L
Li, J
Li, L
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Magill, J
Maldera, S
Manfreda, A
Mayer, M
Mazziotta, MN
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monzani, ME
Morselli, A
Murgia, S
Nuss, E
Omodei, N
Orlando, E
Ormes, JF
Paneque, D
Perkins, JS
Pesce-Rollins, M
Petrosian, V
Piron, F
Pivato, G
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Reposeur, T
Sgro, C
Siskind, EJ
Spada, F
Spandre, G
Spinelli, P
Takahashi, H
Thayer, JB
Thompson, DJ
Tibaldo, L
Torres, DF
Tosti, G
Troja, E
Vianello, G
Winer, BL
Wood, KS
Yassine, M
Cerutti, F
Ferrari, A
Sala, PR
AF Ackermann, M.
Ajello, M.
Albert, A.
Atwood, W. B.
Baldini, L.
Barbiellini, G.
Bastieri, D.
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bonino, R.
Bottacini, E.
Bregeon, J.
Bruel, P.
Buehler, R.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Caraveo, P. A.
Cavazzuti, E.
Cecchi, C.
Chekhtman, A.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Costanza, F.
Cuoco, A.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Desiante, R.
Digel, S. W.
Di Venere, L.
Drell, P. S.
Favuzzi, C.
Fegan, S. J.
Focke, W. B.
Franckowiak, A.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Harding, A. K.
Hewitt, J. W.
Horan, D.
Hou, X.
Iafrate, G.
Johannesson, G.
Kamae, T.
Kuss, M.
Larsson, S.
Latronico, L.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Magill, J.
Maldera, S.
Manfreda, A.
Mayer, M.
Mazziotta, M. N.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Murgia, S.
Nuss, E.
Omodei, N.
Orlando, E.
Ormes, J. F.
Paneque, D.
Perkins, J. S.
Pesce-Rollins, M.
Petrosian, V.
Piron, F.
Pivato, G.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Reposeur, T.
Sgro, C.
Siskind, E. J.
Spada, F.
Spandre, G.
Spinelli, P.
Takahashi, H.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Troja, E.
Vianello, G.
Winer, B. L.
Wood, K. S.
Yassine, M.
Cerutti, F.
Ferrari, A.
Sala, P. R.
CA Fermi LAT Collaboration
TI Measurement of the high-energy gamma-ray emission from the Moon with the
Fermi Large Area Telescope
SO PHYSICAL REVIEW D
LA English
DT Article
ID GALACTIC COSMIC-RAYS
AB We have measured the gamma-ray emission spectrum of the Moon using the data collected by the Large Area Telescope onboard the Fermi satellite during its first seven years of operation, in the energy range from 30 MeV up to a few GeV. We have also studied the time evolution of the flux, finding a correlation with the solar activity. We have developed a full Monte Carlo simulation describing the interactions of cosmic rays with the lunar surface. The results of the present analysis can be explained in the framework of this model, where the production of gamma rays is due to the interactions of cosmic-ray proton and helium nuclei with the surface of the Moon. Finally, we have used our simulation to derive the cosmic-ray proton and helium spectra near Earth from the Moon gamma-ray data.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.] DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Albert, A.; Baldini, L.; Blandford, R. D.; Bottacini, E.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Michelson, P. F.; Monzani, M. E.; Omodei, N.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Petrosian, V.; Reimer, A.; Reimer, O.; Thayer, J. B.; Vianello, G.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Albert, A.; Baldini, L.; Blandford, R. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Michelson, P. F.; Monzani, M. E.; Omodei, N.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Petrosian, V.; Reimer, A.; Reimer, O.; Thayer, J. B.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Atwood, W. B.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Chiaro, G.; Rando, R.] Univ Padua, Dipartimento Fis Astron G Galilei, I-35131 Padua, Italy.
[Bellazzini, R.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bissaldi, E.; Caragiulo, M.; Costanza, F.; de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bonino, R.; Cuoco, A.; Desiante, R.; Latronico, L.; Maldera, S.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bonino, R.; Cuoco, A.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[Bregeon, J.; Cohen-Tanugi, J.; Piron, F.; Yassine, M.] Univ Montpellier, CNRS, IN2P3, Lab Univ & Particules Montpellier, F-34095 Montpellier, France.
[Bruel, P.; Fegan, S. J.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ & Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Cutini, S.; Gasparrini, D.] ASI Sci Data Ctr, I-00133 Rome, Italy.
[Cecchi, C.; Ciprini, S.; Cutini, S.; Gasparrini, D.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA.
[Cutini, S.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Roma, Italy.
[D'Ammando, F.] Ist Radioastron, INAF, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Grp Collegato Udine, Sez Trieste, I-33100 Udine, Italy.
[de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento, I-80132 Naples, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Funk, S.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Grenier, I. A.] Univ Paris Diderot, CEA Saclay, CEA IRFU CNRS, Serv Astrophys,Lab AIM, F-91191 Gif Sur Yvette, France.
[Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Guiriec, S.; Harding, A. K.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Guiriec, S.] NASA, Postdoctoral Program Fellow, Greenbelt, MD 20771 USA.
[Hewitt, J. W.] Univ N Florida, Dept Phys, 1 UNF Dr, Jacksonville, FL 32224 USA.
[Hou, X.] Chinese Acad Sci, Yunnan Observ, Kunming 650216, Peoples R China.
[Hou, X.] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650216, Peoples R China.
[Iafrate, G.] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Kamae, T.] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
[Larsson, S.; Li, L.] KTH Royal Inst Technol, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
[Larsson, S.; Li, L.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Li, J.; Torres, D. F.] Inst Space Sci IEEC CSIC, Campus UAB, E-08193 Barcelona, Spain.
[Magill, J.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Magill, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mitthumsiri, W.] Mahidol Univ, Fac Sci, Dept Phys, Bangkok 10400, Thailand.
[Mizuno, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Murgia, S.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Razzano, M.] Univ & Res MIUR, Italian Minist Educ, FIRB RBFR12PM1F 2012, Rome, Italy.
[Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, BP120, F-33175 Gradignan, France.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Tibaldo, L.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Torres, D. F.] ICREA, E-08010 Barcelona, Spain.
[Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Dept Phys, Columbus, OH 43210 USA.
[Cerutti, F.; Ferrari, A.] European Org Nucl Res CERN, CH-1211 Geneva, Switzerland.
[Sala, P. R.] Ist Nazl Fis Nucl, Sez Milano, I-20133 Milan, Italy.
RP Loparco, F; Mazziotta, MN (reprint author), Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.; Loparco, F (reprint author), Univ & Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
EM loparco@ba.infn.it; mazziotta@ba.infn.it
RI Bissaldi, Elisabetta/K-7911-2016; Reimer, Olaf/A-3117-2013; Orlando,
E/R-5594-2016; sala, paola/E-2868-2013; Funk, Stefan/B-7629-2015;
Bonino, Raffaella/S-2367-2016; Di Venere, Leonardo/C-7619-2017;
OI Bissaldi, Elisabetta/0000-0001-9935-8106; Reimer,
Olaf/0000-0001-6953-1385; sala, paola/0000-0001-9859-5564; Funk,
Stefan/0000-0002-2012-0080; Di Venere, Leonardo/0000-0003-0703-824X;
Mazziotta, Mario Nicola/0000-0001-9325-4672; Sgro',
Carmelo/0000-0001-5676-6214; Pesce-Rollins, Melissa/0000-0003-1790-8018;
Torres, Diego F./0000-0002-1522-9065
FU National Aeronautics and Space Administration in the United States;
Department of Energy in the United States; Commissariat a l'Energie
Atomique in France; Centre National de la Recherche
Scientifique/Institut National de Physique Nucleaire et de Physique des
Particules in France; Agenzia Spaziale Italiana in Italy; Istituto
Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture,
Sports, Science and Technology (MEXT) in Japan; High Energy Accelerator
Research Organization (KEK) in Japan; Japan Aerospace Exploration Agency
(JAXA) in Japan; K. A. Wallenberg Foundation in Sweden; Swedish Research
Council in Sweden; Swedish National Space Board in Sweden; Istituto
Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in
France
FX The Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States; the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France; the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy; the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK), and Japan Aerospace Exploration
Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish
Research Council, and the Swedish National Space Board in Sweden.
Additional support for science analysis during the operations phase from
the Istituto Nazionale di Astrofisica in Italy and the Centre National
d'Etudes Spatiales in France is gratefully acknowledged. The authors
acknowledge the use of HEALPix (http://healpix.jpl.nasa.gov/) described
in Ref. [16].
NR 41
TC 2
Z9 2
U1 5
U2 7
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD APR 8
PY 2016
VL 93
IS 8
AR 082001
DI 10.1103/PhysRevD.93.082001
PG 15
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DI6BT
UT WOS:000373584900002
ER
PT J
AU Jayasekara, C
Premaratne, M
Gunapala, SD
Stockman, MI
AF Jayasekara, Charith
Premaratne, Malin
Gunapala, Sarath D.
Stockman, Mark I.
TI MoS2 spaser
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID LOSS COMPENSATION; MIE SCATTERING; COHERENT-LIGHT; PLASMONICS;
METAMATERIALS; NANOSPHERES; NANOLASER; THRESHOLD; GRAPHENE; NANO
AB We present a comprehensive analysis of a spaser made of a circular shaped highly doped molybdenum disulfide (MoS2) resonator. "Spaser" is an acronym for "surface plasmon amplification by stimulated emission of radiation"-a nanoscale source of surface plasmons generated by stimulated emission in a plasmonic resonator which receives energy nonradiatively. By considering localized surface plasmon modes, operation characteristics of the model are analysed, and tunability of the design is demonstrated. We find the optimum geometric and material parameters of the spaser that provides efficient outputs and carryout a comparative analysis with a similar circular spaser made of graphene. Owing to physical and chemical properties of MoS2 and the active medium, the proposed design delivers efficient outputs in terms of spaser mode energy, operating thresholds, Q-factor, and electric field amplitude. Lower operating thresholds and higher mode energies are notable advantages of the design. Owing to having many superior features to existing similar designs, this MoS2 spaser may be much suited for applications in nanoplasmonic devices. (C) 2016 AIP Publishing LLC.
C1 [Jayasekara, Charith; Premaratne, Malin] Monash Univ, Dept Elect & Comp Syst Engn, Adv Comp & Simulat Lab AxL, Clayton, Vic 3800, Australia.
[Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stockman, Mark I.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
RP Jayasekara, C (reprint author), Monash Univ, Dept Elect & Comp Syst Engn, Adv Comp & Simulat Lab AxL, Clayton, Vic 3800, Australia.
EM charith.jayasekara@monash.edu
OI Jayasekara, Charith/0000-0001-6897-984X; Stockman,
Mark/0000-0002-6996-0806; Premaratne, Malin/0000-0002-2419-4431
FU Monash Institute of Graduate Research (MIGR); Australian Research
Council [DP140100883]
FX The work of Charith Jayasekara was supported by the Monash Institute of
Graduate Research (MIGR). M. Premaratne, S. D. Gunapala, and M. I.
Stockman gratefully acknowledge the financial support from the
Australian Research Council Discovery Grant No. DP140100883.
NR 46
TC 2
Z9 2
U1 9
U2 40
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-8979
EI 1089-7550
J9 J APPL PHYS
JI J. Appl. Phys.
PD APR 7
PY 2016
VL 119
IS 13
AR 133101
DI 10.1063/1.4945378
PG 8
WC Physics, Applied
SC Physics
GA DJ4BK
UT WOS:000374150200001
ER
PT J
AU Belov, K
Mulrey, K
Romero-Wolf, A
Wissel, SA
Zilles, A
Bechtol, K
Borch, K
Chen, P
Clem, J
Gorham, PW
Hast, C
Huege, T
Hyneman, R
Jobe, K
Kuwatani, K
Lam, J
Liu, TC
Nam, J
Naudet, C
Nichol, RJ
Rauch, BF
Rotter, B
Saltzberg, D
Schoorlemmer, H
Seckel, D
Strutt, B
Vieregg, AG
Williams, C
AF Belov, K.
Mulrey, K.
Romero-Wolf, A.
Wissel, S. A.
Zilles, A.
Bechtol, K.
Borch, K.
Chen, P.
Clem, J.
Gorham, P. W.
Hast, C.
Huege, T.
Hyneman, R.
Jobe, K.
Kuwatani, K.
Lam, J.
Liu, T. C.
Nam, J.
Naudet, C.
Nichol, R. J.
Rauch, B. F.
Rotter, B.
Saltzberg, D.
Schoorlemmer, H.
Seckel, D.
Strutt, B.
Vieregg, A. G.
Williams, C.
CA T-510 Collaboration
TI Accelerator Measurements of Magnetically Induced Radio Emission from
Particle Cascades with Applications to Cosmic-Ray Air Showers
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID NEUTRINO DETECTION; PULSES; ENERGY; CHARGE; SIMULATIONS; RADIATION;
CODALEMA; COREAS; LOFAR; MHZ
AB For 50 years, cosmic-ray air showers have been detected by their radio emission. We present the first laboratory measurements that validate electrodynamics simulations used in air shower modeling. An experiment at SLAC provides a beam test of radio-frequency (rf) radiation from charged particle cascades in the presence of a magnetic field, a model system of a cosmic-ray air shower. This experiment provides a suite of controlled laboratory measurements to compare to particle-level simulations of rf emission, which are relied upon in ultrahigh-energy cosmic-ray air shower detection. We compare simulations to data for intensity, linearity with magnetic field, angular distribution, polarization, and spectral content. In particular, we confirm modern predictions that the magnetically induced emission in a dielectric forms a cone that peaks at the Cherenkov angle and show that the simulations reproduce the data within systematic uncertainties.
C1 [Belov, K.; Wissel, S. A.; Borch, K.; Hyneman, R.; Kuwatani, K.; Lam, J.; Saltzberg, D.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Belov, K.; Romero-Wolf, A.; Naudet, C.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Mulrey, K.; Clem, J.; Seckel, D.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Wissel, S. A.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA.
[Zilles, A.] Karlsruher Inst Technol, Inst Expt Kernphys, D-76128 Karlsruhe, Germany.
[Bechtol, K.; Vieregg, A. G.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Chen, P.; Liu, T. C.; Nam, J.] Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys, Grad Inst Astrophys, Dept Phys, Taipei 10617, Taiwan.
[Gorham, P. W.; Rotter, B.; Schoorlemmer, H.] Univ Hawaii, Dept Phys & Astron, Manoa, HI 96822 USA.
[Hast, C.; Jobe, K.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Huege, T.] Karlsruher Inst Technol, Inst Kernphys, D-76021 Karlsruhe, Germany.
[Hyneman, R.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Nichol, R. J.] UCL, Dept Phys & Astron, Mortimer St, London WC1E 6BT, England.
[Rauch, B. F.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Vieregg, A. G.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA.
[Williams, C.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
RP Wissel, SA (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.; Wissel, SA (reprint author), Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA.
EM swissel@physics.ucla.edu
FU Department of Energy [DE-AC02-76SF00515, DE-SC0009937]; National
Aeronautics and Space Administration; Taiwan Ministry of Science and
Technology [MOST103-2119-M-002-002]; JPL Internal Research and
Technology Development program; Kavli Institute for Cosmological Physics
at the University of Chicago [NSF PHY-1125897]; Karlsruher Institut fur
Technologie; SLAC National Accelerator Laboratory
FX We thank the referees for critical remarks leading to an improved
presentation. The authors thank SLAC National Accelerator Laboratory for
providing facilities and support and especially Janice Nelson and Carl
Hudspeth for their support and dedication that made T-510 possible. We
thank D. Z. Besson for helpful discussions. This material is based upon
work supported by the Department of Energy under Awards No.
DE-AC02-76SF00515, No. DE-SC0009937, and others. This work was supported
in part by grants from the National Aeronautics and Space Administration
and the Taiwan Ministry of Science and Technology under Project No.
MOST103-2119-M-002-002, among others. Part of this research was funded
through the JPL Internal Research and Technology Development program.
This work was supported in part by the Kavli Institute for Cosmological
Physics at the University of Chicago through Grant No. NSF PHY-1125897
and an endowment from the Kavli Foundation and its founder Fred Kavli.
K. Belov acknowledges support from the Karlsruher Institut fur
Technologie under a guest fellowship. We are grateful to the ANITA
Collaboration for use of antennas and other equipment.
NR 41
TC 1
Z9 1
U1 2
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 7
PY 2016
VL 116
IS 14
AR 141103
DI 10.1103/PhysRevLett.116.141103
PG 6
WC Physics, Multidisciplinary
SC Physics
GA DI6CT
UT WOS:000373587500005
PM 27104694
ER
PT J
AU Louvat, P
Bonifacie, M
Giunta, T
Michel, A
Coleman, M
AF Louvat, Pascale
Bonifacie, Magali
Giunta, Thomas
Michel, Agnes
Coleman, Max
TI Determination of Bromine Stable Isotope Ratios from Saline Solutions by
"Wet Plasma" MC-ICPMS Including a Comparison between High- and
Low-Resolution Modes, and Three Introduction Systems
SO ANALYTICAL CHEMISTRY
LA English
DT Article
ID MASS-SPECTROMETRY; FORMATION WATER; CHLORINE; ORIGIN; DELTA-BR-81;
DELTA-CL-37; SAMPLES
AB We describe a novel method for measuring stable bromine isotope compositions in saline solutions such as seawater, brines, and formation waters. Bromine is extracted from the samples by ion exchange chromatography on anion exchange resin AG 1-X4 with NH4NO3 and measured by MC-ICP-MS in wet plasma conditions. Sample introduction through a small spray chamber provided good sensitivity and stability of the Br signal compared to direct injection (d-DIHEN) and desolvation (APEX). NH4NO3 media allowed fast (<3 min) washing of the system. Despite Ar2H+ spectral interference on Br-81(+), for the first time low-resolution mode (with appropriate tuning of Ar2H+/Br-81(+) sensitivity) gave higher precision Br-81/Br-79 measurements than high-resolution (HR), due to the narrowness of the Br-81(+) plateau in HR mode and to slight mass drifting with time. Additionally, 1 mu g Br is the lower amount needed for a triplicate determination of delta Br-81 by MC-ICP-MS, with reproducibility often < +/- 0.1% (2 SD). Four HBr solutions were prepared by evaporation/condensation in order to obtain in-house reference solutions with 3% variations in delta Br-81 and to assess the reproducibility and accuracy of the method. Long-term (>3 years) reproducibility between +/- 0.11 and +/- 0.27% (2 SD) was obtained for the four HBr solutions, the international standard reference material NIST SRM 977 (delta Br-81(SMOB) = -0.65 +/- 1.1%, 1 SD), and seawaters (synthetic and natural). The accuracy of the MC-ICP-MS method was validated by comparing the delta Br-81 obtained for these solutions with dual-inlet IRMS measurements on CH3Br gas. Finally, the method was successfully applied to 22 natural samples.
C1 [Louvat, Pascale; Bonifacie, Magali; Giunta, Thomas; Michel, Agnes] Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, UMR CNRS 7154, F-75238 Paris 05, France.
[Bonifacie, Magali] Inst Phys Globe Paris, Observ Volcanol & Sismol Guadeloupe, F-97113 Le Houelmont, Gourbeyre Guade, France.
[Coleman, Max] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
RP Louvat, P (reprint author), Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, UMR CNRS 7154, F-75238 Paris 05, France.
EM louvat@ipgp.fr
RI Louvat, Pascale/E-8907-2017
OI Louvat, Pascale/0000-0003-1972-0633
FU PTeV (Programme Transverse en Volcanologie); multidisciplinary program
PART of IPGP/region Ile de France (SESAME) [12015908]; CNRS INSU ALEAS
program; Invited Professor program of Universite Paris Diderot; Jet
Propulsion Laboratory (JPL), California Institute of Technology
FX PL and MB were funded by PTeV (Programme Transverse en Volcanologie),
multidisciplinary program PART of IPGP/region Ile de France (SESAME
Grant no. 12015908), and CNRS INSU ALEAS program. MC was partly funded
by both the Invited Professor program of Universite Paris Diderot and
the Jet Propulsion Laboratory (JPL), California Institute of Technology,
under contract with the National Aeronautics and Space Administration
(NASA). Assya and Abdellah Krim are thanked for their help in
calibrating ion exchange chromatography. This is IPGP contribution
number 3712.
NR 24
TC 0
Z9 0
U1 4
U2 15
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0003-2700
EI 1520-6882
J9 ANAL CHEM
JI Anal. Chem.
PD APR 5
PY 2016
VL 88
IS 7
BP 3891
EP 3898
DI 10.1021/acs.analchem.6b00062
PG 8
WC Chemistry, Analytical
SC Chemistry
GA DI7CI
UT WOS:000373656300064
PM 26898343
ER
PT J
AU van Donkelaar, A
Martin, RV
Brauer, M
Hsu, NC
Kahn, RA
Levy, RC
Lyapustin, A
Sayer, AM
Winker, DM
AF van Donkelaar, Aaron
Martin, Randall V.
Brauer, Michael
Hsu, N. Christina
Kahn, Ralph A.
Levy, Robert C.
Lyapustin, Alexei
Sayer, Andrew M.
Winker, David M.
TI Global Estimates of Fine Particulate Matter using a Combined
Geophysical-Statistical Method with Information from Satellites, Models,
and Monitors
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID AEROSOL OPTICAL DEPTH; GEOGRAPHICALLY WEIGHTED REGRESSION;
UNITED-STATES; CARBONACEOUS AEROSOLS; EXPOSURE ASSESSMENT;
NORTH-AMERICA; MODIS; PRODUCTS; PM2.5; LAND
AB We estimated global fine particulate matter (PM2.5) concentrations using information from satellite-, simulation- and monitor-based sources by applying a Geographically Weighted Regression (GWR) to global geophysically based satellite-derived PM2.5 estimates. Aerosol optical depth from multiple satellite products (MISR, MODIS Dark Target, MODIS and SeaWiFS Deep Blue, and MODIS MAIAC) was combined with simulation (GEOS-Chem) based upon their relative uncertainties as determined using ground-based sun photometer (AERONET) observations for 1998-2014. The GWR predictors included simulated aerosol composition and land use information. The resultant PM2.5 estimates were highly consistent (R-2 = 0.81) with out-of-sample cross-validated PM2.5 concentrations from monitors. The global population-weighted annual average PM2.5 concentrations were 3-fold higher than the 10 mu g/m(3) WHO guideline, driven by exposures in Asian and African regions. Estimates in regions with high contributions from mineral dust were associated with higher uncertainty, resulting from both sparse ground-based monitoring, and challenging conditions for retrieval and simulation. This approach demonstrates that the addition of even sparse ground-based measurements to more globally continuous PM2.5 data sources can yield valuable improvements to PM2.5 characterization on a global scale.
C1 [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Brauer, Michael] Univ British Columbia, Sch Populat & Publ Hlth, 2206 East Mall, Vancouver, BC V6T 1Z3, Canada.
[Hsu, N. Christina; Kahn, Ralph A.; Levy, Robert C.; Lyapustin, Alexei; Sayer, Andrew M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lyapustin, Alexei; Sayer, Andrew M.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Greenbelt, MD 20771 USA.
[Winker, David M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP van Donkelaar, A (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
EM Aaron.van.Donkelaar@dal.ca
RI Sayer, Andrew/H-2314-2012; Levy, Robert/M-7764-2013; Martin,
Randall/C-1205-2014; Chem, GEOS/C-5595-2014
OI Sayer, Andrew/0000-0001-9149-1789; Levy, Robert/0000-0002-8933-5303;
Martin, Randall/0000-0003-2632-8402;
FU Natural Science and Engineering Research Council of Canada; NASA
MEaSUREs program; NASA EOS program
FX We are grateful to the MODIS, MISR, SeaWiFS, CALIOP, and AERONET teams
that have made this work possible through the creation, validation, and
public release of their data products, as well as Compute Canada for
computing resources. This work was supported by the Natural Science and
Engineering Research Council of Canada. SeaWiFS and MODIS Deep Blue data
set development was supported by the NASA MEaSUREs and EOS programs,
respectively.
NR 52
TC 14
Z9 14
U1 30
U2 51
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
EI 1520-5851
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD APR 5
PY 2016
VL 50
IS 7
BP 3762
EP 3772
DI 10.1021/acs.est.5b05833
PG 11
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA DI7CD
UT WOS:000373655800055
PM 26953851
ER
PT J
AU Lee, HJ
Son, YS
AF Lee, Hyung Joo
Son, Youn-Suk
TI Spatial Variability of AERONET Aerosol Optical Properties and Satellite
Data in South Korea during NASA DRAGON-Asia Campaign
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID OZONE MONITORING INSTRUMENT; SOURCE APPORTIONMENT; SEOUL; DUST;
RETRIEVAL; PARTICLES; ALGORITHM; EMISSIONS; TRENDS; PM2.5
AB We investigated spatial variability in aerosol optical properties, including aerosol optical depth (AOD), fine-mode fraction (FMF), and single scattering albedo (SSA), observed at 21 Aerosol Robotic Network (AERONET) sites and satellite remote sensing data in South Korea during the spring of 2012. These dense AERONET networks established in a National Aeronautics and Space Administration (NASA) field campaign enabled us to examine the spatially detailed aerosol size distribution and composition as well as aerosol levels. The springtime particle air quality was characterized by high background aerosol levels and high contributions of coarse-mode aerosols to total aerosols. We found that between-site correlations and coefficient of divergence for AOD and FMF strongly relied on the distance between sites, particularly in the south north direction. Higher AOD was related to higher population density and lower distance from highways, and the aerosol size distribution and composition reflected source-specific characteristics. The ratios of satellite NO2 to AOD, which indicate the relative contributions of local combustion sources to aerosol levels, represented higher local contributions in metropolitan Seoul and Pusan. Our study demonstrates that the aerosol levels were determined by both local and regional pollution and that the relative contributions of these pollutions to aerosols generated spatial heterogeneity in the particle air quality.
C1 [Lee, Hyung Joo] NASA, Postdoctoral Program, Div Earth Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Son, Youn-Suk] Korea Atom Energy Res Inst, Res Div Ind & Environm, Jeongeup Si 580185, Jeollabuk Do, South Korea.
RP Lee, HJ (reprint author), NASA, Postdoctoral Program, Div Earth Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM hyungjoo.lee@nasa.gov
FU NASA Postdoctoral Program at the Ames Research Center; NASA
FX H.J.L. was supported by an appointment to the NASA Postdoctoral Program
at the Ames Research Center, administered by Oak Ridge Associated
Universities through a contract with NASA. The authors thank the
principal investigators and their staff for establishing and maintaining
the AERONET sites used in this study. We also appreciate the MODIS and
OMI science teams for providing their satellite data. The authors
gratefully acknowledge the NOAA Air Resources Laboratory (ARL) for the
provision of the HYSPLIT transport and dispersion model and/or READY
website (http://www.ready.noaa.gov) used in this publication.
NR 39
TC 0
Z9 0
U1 4
U2 13
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
EI 1520-5851
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD APR 5
PY 2016
VL 50
IS 7
BP 3954
EP 3964
DI 10.1021/acs.est.5b04831
PG 11
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA DI7CD
UT WOS:000373655800078
PM 26953969
ER
PT J
AU Mozer, FS
Agapitov, OA
Artemyev, A
Burch, JL
Ergun, RE
Giles, BL
Mourenas, D
Torbert, RB
Phan, TD
Vasko, I
AF Mozer, F. S.
Agapitov, O. A.
Artemyev, A.
Burch, J. L.
Ergun, R. E.
Giles, B. L.
Mourenas, D.
Torbert, R. B.
Phan, T. D.
Vasko, I.
TI Magnetospheric Multiscale Satellite Observations of Parallel Electron
Acceleration in Magnetic Field Reconnection by Fermi Reflection from
Time Domain Structures
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID SOLITARY WAVES; MAGNETOTAIL; GEOTAIL; REGION; HOLES
AB The same time domain structures (TDS) have been observed on two Magnetospheric Multiscale Satellites near Earth's dayside magnetopause. These TDS, traveling away from the X line along the magnetic field at 4000 km/s, accelerated field-aligned similar to 5 eV electrons to similar to 200 eV by a single Fermi reflection of the electrons by these overtaking barriers. Additionally, the TDS contained both positive and negative potentials, so they were a mixture of electron holes and double layers. They evolve in similar to 10 km of space or 7 ms of time and their spatial scale size is 10-20 km, which is much larger than the electron gyroradius (< 1 km) or the electron inertial length (4 km at the observation point, less nearer the X line).
C1 [Mozer, F. S.; Agapitov, O. A.; Phan, T. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Agapitov, O. A.] Taras Shevchenko Natl Univ Kyiv, Glushkova Ave 4, UA-01601 Kiev, Ukraine.
[Artemyev, A.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90002 USA.
[Burch, J. L.] SW Res Inst, San Antonio, TX 78238 USA.
[Ergun, R. E.] Univ Colorado, LASP, Boulder, CO 80303 USA.
[Giles, B. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mourenas, D.] Univ Orleans, E CNRS LPC2, F-45100 Orleans, France.
[Torbert, R. B.] Univ New Hampshire, Durham, NH 03824 USA.
[Vasko, I.] Russian Acad Sci, Space Res Inst, Moscow 117342, Russia.
RP Mozer, FS (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM forrest.mozer@gmail.com
RI NASA MMS, Science Team/J-5393-2013; Agapitov, Oleksiy/F-9636-2010
OI NASA MMS, Science Team/0000-0002-9504-5214;
FU NASA [NNX08AO83]; JHU/APL [922613]; Dmitry Zimin Dynasty Foundation;
Presidental Grant [MK-7757.2016.2]; NASA at SwRI [NNG04EB99 C]
FX The authors thank V. Krasnoselskikh for several useful comments and
suggestions. We are deeply indebted to the entire MMS team that built
such wonderful instruments and an outstanding program. The work of F. S.
M. and T. D. P. was supported by NASA Grant No. NNX08AO83 J. L. B., R.
B. T., and B. L. G. were supported by NASA Contract No. NNG04EB99 C at
SwRI. The work of O. A. A. and F. S. M. was also supported under JHU/APL
Contract No. 922613 (RBSP-EFW). A. A. is grateful to the Dmitry Zimin
Dynasty Foundation for support. The work of I. V. was supported by the
Presidental Grant No. MK-7757.2016.2.
NR 33
TC 6
Z9 6
U1 1
U2 10
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 5
PY 2016
VL 116
IS 14
AR 145101
DI 10.1103/PhysRevLett.116.145101
PG 5
WC Physics, Multidisciplinary
SC Physics
GA DI6CQ
UT WOS:000373587200003
PM 27104714
ER
PT J
AU Aartsen, MG
Abraham, K
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Ahrens, M
Altmann, D
Anderson, T
Ansseau, I
Anton, G
Archinger, M
Arguelles, C
Arlen, TC
Auffenberg, J
Bai, X
Barwick, SW
Baum, V
Bay, R
Beatty, JJ
Tjus, JB
Becker, KH
Beiser, E
BenZvi, S
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Besson, DZ
Binder, G
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Borner, M
Bos, F
Bose, D
Boser, S
Botner, O
Braun, J
Brayeur, L
Bretz, HP
Buzinsky, N
Casey, J
Casier, M
Cheung, E
Chirkin, D
Christov, A
Clark, K
Classen, L
Coenders, S
Collin, GH
Conrad, JM
Cowen, DF
Silva, AHC
Danninger, M
Daughhetee, J
Davis, JC
Day, M
de Andre, JPAM
De Clercq, C
Rosendo, ED
Dembinski, H
De Ridder, S
Desiati, P
de Vries, KD
de Wasseige, G
de With, M
DeYoung, T
Diaz-Velez, JC
di Lorenzo, V
Dumm, JP
Dunkman, M
Eberhardt, B
Edsjo, J
Ehrhardt, T
Eichmann, B
Euler, S
Evenson, PA
Fahey, S
Fazely, AR
Feintzeig, J
Felde, J
Filimonov, K
Finley, C
Flis, S
Fosig, CC
Fuchs, T
Gaisser, TK
Gaior, R
Gallagher, J
Gerhardt, L
Ghorbani, K
Gier, D
Gladstone, L
Glagla, M
Glusenkamp, T
Goldschmidt, A
Golup, G
Gonzalez, JG
Gora, D
Grant, D
Griffith, Z
Gross, A
Ha, C
Haack, C
Ismail, AH
Hallgren, A
Halzen, F
Hansen, E
Hansmann, B
Hanson, K
Hebecker, D
Heereman, D
Helbing, K
Hellauer, R
Hickford, S
Hignight, J
Hill, GC
Hoffman, KD
Hoffmann, R
Holzapfel, K
Homeier, A
Hoshina, K
Huang, F
Huber, M
Huelsnitz, W
Hulth, PO
Hultqvist, K
In, S
Ishihara, A
Jacobi, E
Japaridze, GS
Jeong, M
Jero, K
Jones, BJP
Jurkovic, M
Kappes, A
Karg, T
Karle, A
Katz, U
Kauer, M
Keivani, A
Kelley, JL
Kemp, J
Kheirandish, A
Kiryluk, J
Klein, SR
Kohnen, G
Koirala, R
Kolanoski, H
Konietz, R
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krings, K
Kroll, G
Kroll, M
Kruckl, G
Kunnen, J
Kurahashi, N
Kuwabara, T
Labare, M
Lanfranchi, JL
Larson, MJ
Lesiak-Bzdak, M
Leuermann, M
Leuner, J
Lu, L
Lunemann, J
Madsen, J
Maggi, G
Mahn, KBM
Mandelartz, M
Maruyama, R
Mase, K
Matis, HS
Maunu, R
McNally, F
Meagher, K
Medici, M
Meier, M
Meli, A
Menne, T
Merino, G
Meures, T
Miarecki, S
Middell, E
Mohrmann, L
Montaruli, T
Morse, R
Nahnhauer, R
Naumann, U
Neer, G
Niederhausen, H
Nowicki, SC
Nygren, DR
Pollmann, AO
Olivas, A
Omairat, A
O'Murchadha, A
Palczewski, T
Pandya, H
Pankova, DV
Paul, L
Pepper, JA
de los Heros, CP
Pfendner, C
Pieloth, D
Pinat, E
Posselt, J
Price, PB
Przybylski, GT
Quinnan, M
Raab, C
Radel, L
Rameez, M
Rawlins, K
Reimann, R
Relich, M
Resconi, E
Rhode, W
Richman, M
Richter, S
Riedel, B
Robertson, S
Rongen, M
Rott, C
Ruhe, T
Ryckbosch, D
Sabbatini, L
Sander, HG
Sandrock, A
Sandroos, J
Sarkar, S
Savage, C
Schatto, K
Schimp, M
Schlunder, P
Schmidt, T
Schoenen, S
Schoneberg, S
Schonwald, A
Schulte, L
Schumacher, L
Scott, P
Seckel, D
Seunarine, S
Silverwood, H
Soldin, D
Song, M
Spiczak, GM
Spiering, C
Stahlberg, M
Stamatikos, M
Stanev, T
Stasik, A
Steuer, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strom, R
Strotjohann, NL
Sullivan, GW
Sutherland, M
Taavola, H
Taboada, I
Tatar, J
Ter-Antonyan, S
Terliuk, A
Tesic, G
Tilav, S
Toale, PA
Tobin, MN
Toscano, S
Tosi, D
Tselengidou, M
Turcati, A
Unger, E
Usner, M
Vallecorsa, S
Vandenbroucke, J
van Eijndhoven, N
Vanheule, S
van Santen, J
Veenkamp, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Wallace, A
Wallraff, M
Wandkowsky, N
Weaver, C
Wendt, C
Westerhoff, S
Whelan, BJ
Wiebe, K
Wiebusch, CH
Wille, L
Williams, DR
Wills, L
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, DL
Xu, XW
Xu, Y
Yanez, JP
Yodh, G
Yoshida, S
Zoll, M
AF Aartsen, M. G.
Abraham, K.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Ahrens, M.
Altmann, D.
Anderson, T.
Ansseau, I.
Anton, G.
Archinger, M.
Arguelles, C.
Arlen, T. C.
Auffenberg, J.
Bai, X.
Barwick, S. W.
Baum, V.
Bay, R.
Beatty, J. J.
Tjus, J. Becker
Becker, K. -H.
Beiser, E.
BenZvi, S.
Berghaus, P.
Berley, D.
Bernardini, E.
Bernhard, A.
Besson, D. Z.
Binder, G.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Boerner, M.
Bos, F.
Bose, D.
Boeser, S.
Botner, O.
Braun, J.
Brayeur, L.
Bretz, H. -P.
Buzinsky, N.
Casey, J.
Casier, M.
Cheung, E.
Chirkin, D.
Christov, A.
Clark, K.
Classen, L.
Coenders, S.
Collin, G. H.
Conrad, J. M.
Cowen, D. F.
Silva, A. H. Cruz
Danninger, M.
Daughhetee, J.
Davis, J. C.
Day, M.
de Andre, J. P. A. M.
De Clercq, C.
Rosendo, E. del Pino
Dembinski, H.
De Ridder, S.
Desiati, P.
de Vries, K. D.
de Wasseige, G.
de With, M.
DeYoung, T.
Diaz-Velez, J. C.
di Lorenzo, V.
Dumm, J. P.
Dunkman, M.
Eberhardt, B.
Edsjo, J.
Ehrhardt, T.
Eichmann, B.
Euler, S.
Evenson, P. A.
Fahey, S.
Fazely, A. R.
Feintzeig, J.
Felde, J.
Filimonov, K.
Finley, C.
Flis, S.
Foesig, C. -C.
Fuchs, T.
Gaisser, T. K.
Gaior, R.
Gallagher, J.
Gerhardt, L.
Ghorbani, K.
Gier, D.
Gladstone, L.
Glagla, M.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Gonzalez, J. G.
Gora, D.
Grant, D.
Griffith, Z.
Gross, A.
Ha, C.
Haack, C.
Ismail, A. Haj
Hallgren, A.
Halzen, F.
Hansen, E.
Hansmann, B.
Hanson, K.
Hebecker, D.
Heereman, D.
Helbing, K.
Hellauer, R.
Hickford, S.
Hignight, J.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Holzapfel, K.
Homeier, A.
Hoshina, K.
Huang, F.
Huber, M.
Huelsnitz, W.
Hulth, P. O.
Hultqvist, K.
In, S.
Ishihara, A.
Jacobi, E.
Japaridze, G. S.
Jeong, M.
Jero, K.
Jones, B. J. P.
Jurkovic, M.
Kappes, A.
Karg, T.
Karle, A.
Katz, U.
Kauer, M.
Keivani, A.
Kelley, J. L.
Kemp, J.
Kheirandish, A.
Kiryluk, J.
Klein, S. R.
Kohnen, G.
Koirala, R.
Kolanoski, H.
Konietz, R.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Krings, K.
Kroll, G.
Kroll, M.
Krueckl, G.
Kunnen, J.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Lanfranchi, J. L.
Larson, M. J.
Lesiak-Bzdak, M.
Leuermann, M.
Leuner, J.
Lu, L.
Lunemann, J.
Madsen, J.
Maggi, G.
Mahn, K. B. M.
Mandelartz, M.
Maruyama, R.
Mase, K.
Matis, H. S.
Maunu, R.
McNally, F.
Meagher, K.
Medici, M.
Meier, M.
Meli, A.
Menne, T.
Merino, G.
Meures, T.
Miarecki, S.
Middell, E.
Mohrmann, L.
Montaruli, T.
Morse, R.
Nahnhauer, R.
Naumann, U.
Neer, G.
Niederhausen, H.
Nowicki, S. C.
Nygren, D. R.
Pollmann, A. Obertacke
Olivas, A.
Omairat, A.
O'Murchadha, A.
Palczewski, T.
Pandya, H.
Pankova, D. V.
Paul, L.
Pepper, J. A.
de los Heros, C. Perez
Pfendner, C.
Pieloth, D.
Pinat, E.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Quinnan, M.
Raab, C.
Raedel, L.
Rameez, M.
Rawlins, K.
Reimann, R.
Relich, M.
Resconi, E.
Rhode, W.
Richman, M.
Richter, S.
Riedel, B.
Robertson, S.
Rongen, M.
Rott, C.
Ruhe, T.
Ryckbosch, D.
Sabbatini, L.
Sander, H. -G.
Sandrock, A.
Sandroos, J.
Sarkar, S.
Savage, C.
Schatto, K.
Schimp, M.
Schlunder, P.
Schmidt, T.
Schoenen, S.
Schoeneberg, S.
Schoenwald, A.
Schulte, L.
Schumacher, L.
Scott, P.
Seckel, D.
Seunarine, S.
Silverwood, H.
Soldin, D.
Song, M.
Spiczak, G. M.
Spiering, C.
Stahlberg, M.
Stamatikos, M.
Stanev, T.
Stasik, A.
Steuer, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strom, R.
Strotjohann, N. L.
Sullivan, G. W.
Sutherland, M.
Taavola, H.
Taboada, I.
Tatar, J.
Ter-Antonyan, S.
Terliuk, A.
Tesic, G.
Tilav, S.
Toale, P. A.
Tobin, M. N.
Toscano, S.
Tosi, D.
Tselengidou, M.
Turcati, A.
Unger, E.
Usner, M.
Vallecorsa, S.
Vandenbroucke, J.
van Eijndhoven, N.
Vanheule, S.
van Santen, J.
Veenkamp, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Wallace, A.
Wallraff, M.
Wandkowsky, N.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whelan, B. J.
Wiebe, K.
Wiebusch, C. H.
Wille, L.
Williams, D. R.
Wills, L.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, D. L.
Xu, X. W.
Xu, Y.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zoll, M.
CA IceCube Collaboration
TI Improved limits on dark matter annihilation in the Sun with the
79-string IceCube detector and implications for supersymmetry
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE dark matter experiments; dark matter theory; neutrino experiments
AB We present an improved event-level likelihood formalism for including neutrino telescope data in global fits to new physics. We derive limits on spin-dependent dark matter-proton scattering by employing the new formalism in a re-analysis of data from the 79-string IceCube search for dark matter annihilation in the Sun, including explicit energy information for each event. The new analysis excludes a number of models in the weak-scale minimal supersymmetric standard model (MSSM) for the first time. This work is accompanied by the public release of the 79-string IceCube data, as well as an associated computer code for applying the new likelihood to arbitrary dark matter models.
C1 [Auffenberg, J.; Bissok, M.; Blumenthal, J.; Gier, D.; Glagla, M.; Haack, C.; Hansmann, B.; Kemp, J.; Konietz, R.; Leuermann, M.; Leuner, J.; Paul, L.; Raedel, L.; Reimann, R.; Rongen, M.; Schimp, M.; Schoenen, S.; Schumacher, L.; Stahlberg, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Phys Inst 3, D-52056 Aachen, Germany.
[Aartsen, M. G.; Hill, G. C.; Robertson, S.; Wallace, A.; Whelan, B. J.] Univ Adelaide, Dept Phys, Adelaide, SA 5005, Australia.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, 3211 Providence Dr, Anchorage, AK 99508 USA.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Tatar, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Binder, G.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.; Tatar, J.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[de With, M.; Hebecker, D.; Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Tjus, J. Becker; Bos, F.; Eichmann, B.; Kroll, M.; Mandelartz, M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Homeier, A.; Schulte, L.; Voge, M.] Univ Bonn, Phys Inst, Nussallee 12, D-53115 Bonn, Germany.
[Aguilar, J. A.; Ansseau, I.; Heereman, D.; Meagher, K.; Meures, T.; O'Murchadha, A.; Pinat, E.; Raab, C.] Univ Libre Bruxelles, Sci Fac CP230, B-1050 Brussels, Belgium.
[Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; de Wasseige, G.; Golup, G.; Kunnen, J.; Lunemann, J.; Maggi, G.; Toscano, S.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Arguelles, C.; Collin, G. H.; Conrad, J. M.; Jones, B. J. P.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Gaior, R.; Ishihara, A.; Kuwabara, T.; Lu, L.; Mase, K.; Relich, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.; Silverwood, H.] Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch, New Zealand.
[Berley, D.; Blaufuss, E.; Cheung, E.; Felde, J.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Maunu, R.; Olivas, A.; Schmidt, T.; Song, M.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
[Hansen, E.; Koskinen, D. J.; Larson, M. J.; Medici, M.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Boerner, M.; Fuchs, T.; Meier, M.; Menne, T.; Pieloth, D.; Rhode, W.; Ruhe, T.; Sandrock, A.; Schlunder, P.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[de Andre, J. P. A. M.; DeYoung, T.; Hignight, J.; Mahn, K. B. M.; Neer, G.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Buzinsky, N.; Grant, D.; Kopper, C.; Nowicki, S. C.; Riedel, B.; Weaver, Ch.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Altmann, D.; Anton, G.; Classen, L.; Kappes, A.; Katz, U.; Tselengidou, M.] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[De Ridder, S.; Ismail, A. Haj; Labare, M.; Meli, A.; Ryckbosch, D.; Vanheule, S.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[Barwick, S. W.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Ahlers, M.; Beiser, E.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Griffith, Z.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; McNally, F.; Merino, G.; Morse, R.; Richter, S.; Sabbatini, L.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Xu, D. L.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
[Ahlers, M.; Beiser, E.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Griffith, Z.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; McNally, F.; Merino, G.; Morse, R.; Richter, S.; Sabbatini, L.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Xu, D. L.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Archinger, M.; Baum, V.; Boeser, S.; Rosendo, E. del Pino; di Lorenzo, V.; Eberhardt, B.; Ehrhardt, T.; Foesig, C. -C.; Koepke, L.; Kroll, G.; Krueckl, G.; Sander, H. -G.; Sandroos, J.; Schatto, K.; Steuer, A.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, Staudinger Weg 7, D-55099 Mainz, Germany.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Abraham, K.; Bernhard, A.; Coenders, S.; Gross, A.; Holzapfel, K.; Huber, M.; Jurkovic, M.; Krings, K.; Resconi, E.; Turcati, A.; Veenkamp, J.] Tech Univ Munich, D-85748 Garching, Germany.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Koirala, R.; Pandya, H.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Koirala, R.; Pandya, H.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Kauer, M.; Maruyama, R.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, 1 Keble Rd, Oxford OX1 3NP, England.
[Kurahashi, N.; Richman, M.; Wills, L.; Yodh, G.] Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Ahrens, M.; Bohm, C.; Danninger, M.; Dumm, J. P.; Edsjo, J.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Savage, C.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Ahrens, M.; Bohm, C.; Danninger, M.; Dumm, J. P.; Edsjo, J.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Savage, C.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.; Xu, Y.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Bose, D.; In, S.; Jeong, M.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
[Clark, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Palczewski, T.; Pepper, J. A.; Toale, P. A.; Williams, D. R.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Anderson, T.; Arlen, T. C.; Cowen, D. F.; Dunkman, M.; Huang, F.; Keivani, A.; Lanfranchi, J. L.; Pankova, D. V.; Quinnan, M.; Tesic, G.] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA.
[BenZvi, S.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Boersma, D. J.; Botner, O.; Euler, S.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.; Unger, E.] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden.
[Becker, K. -H.; Bindig, D.; Helbing, K.; Hickford, S.; Hoffmann, R.; Kopper, S.; Naumann, U.; Pollmann, A. Obertacke; Omairat, A.; Posselt, J.; Soldin, D.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Karg, T.; Kowalski, M.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stasik, A.; Stoessl, A.; Strotjohann, N. L.; Terliuk, A.; Usner, M.; van Santen, J.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Danninger, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Scott, P.] Imperial Coll London, Dept Phys, London SW7 2AZ, England.
[Silverwood, H.] Univ Amsterdam, GRAPPA Inst, NL-1098 XH Amsterdam, Netherlands.
RP Danninger, M (reprint author), Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.; Danninger, M (reprint author), Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.; Scott, P (reprint author), Imperial Coll London, Dept Phys, London SW7 2AZ, England.
EM matthias.danninger@cern.ch; p.scott@imperial.ac.uk
OI Perez de los Heros, Carlos/0000-0002-2084-5866; Koskinen,
David/0000-0002-0514-5917; Sarkar, Subir/0000-0002-3542-858X;
Strotjohann, Nora Linn/0000-0002-4667-6730; Arguelles Delgado,
Carlos/0000-0003-4186-4182
FU U.S. National Science Foundation-Office of Polar Programs; U.S. National
Science Foundation-Physics Division; University of Wisconsin Alumni
Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid
infrastructure at the University of Wisconsin - Madison; Open Science
Grid (OSG) grid infrastructure; U.S. Department of Energy; National
Energy Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI) grid computing resources; Natural Sciences and
Engineering Research Council of Canada; WestGrid and Compute/Calcul
Canada; Swedish Research Council; Swedish Polar Research Secretariat;
Swedish National Infrastructure for Computing (SNIC); Knut and Alice
Wallenberg Foundation, Sweden; German Ministry for Education and
Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Helmholtz
Alliance for Astroparticle Physics (HAP); Research Department of Plasmas
with Complex Interactions (Bochum), Germany; Fund for Scientific
Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to
encourage scientific and technological research in industry (IWT);
Belgian Federal Science Policy Office (Belspo); University of Oxford,
United Kingdom; Marsden Fund, New Zealand; Australian Research Council;
Japan Society for Promotion of Science (JSPS); Swiss National Science
Foundation (SNSF), Switzerland; National Research Foundation of Korea
(NRF); Danish National Research Foundation, Denmark (DNRF); Science and
Technology Facilities Council, United Kingdom (STFC)
FX We acknowledge the support from the following agencies: U.S. National
Science Foundation-Office of Polar Programs, U.S. National Science
Foundation-Physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin - Madison, the Open Science Grid (OSG)
grid infrastructure; U.S. Department of Energy, and National Energy
Research Scientific Computing Center, the Louisiana Optical Network
Initiative (LONI) grid computing resources; Natural Sciences and
Engineering Research Council of Canada, WestGrid and Compute/Calcul
Canada; Swedish Research Council, Swedish Polar Research Secretariat,
Swedish National Infrastructure for Computing (SNIC), and Knut and Alice
Wallenberg Foundation, Sweden; German Ministry for Education and
Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz
Alliance for Astroparticle Physics (HAP), Research Department of Plasmas
with Complex Interactions (Bochum), Germany; Fund for Scientific
Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to
encourage scientific and technological research in industry (IWT),
Belgian Federal Science Policy Office (Belspo); University of Oxford,
United Kingdom; Marsden Fund, New Zealand; Australian Research Council;
Japan Society for Promotion of Science (JSPS); the Swiss National
Science Foundation (SNSF), Switzerland; National Research Foundation of
Korea (NRF); Danish National Research Foundation, Denmark (DNRF);
Science and Technology Facilities Council, United Kingdom (STFC). We
also thank the GAMBIT DM and Collider Workgroups for code testing of
nulike.
NR 40
TC 20
Z9 20
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD APR
PY 2016
IS 4
AR 022
DI 10.1088/1475-7516/2016/04/022
PG 31
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA EJ5VI
UT WOS:000393286400001
ER
PT J
AU Ding, YN
Carton, JA
Chepurin, GA
Steele, M
Hakkinen, S
AF Ding, Yanni
Carton, James A.
Chepurin, Gennady A.
Steele, Michael
Hakkinen, Sirpa
TI Seasonal heat and freshwater cycles in the Arctic Ocean in CMIP5 coupled
models
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID INTERCOMPARISON PROJECT; CLIMATE; ICE; VARIABILITY; REANALYSIS;
ATLANTIC; REGIMES; SYSTEM
AB This study examines the processes governing the seasonal response of the Arctic Ocean and sea ice to surface forcings as they appear in historical simulations of 14 Coupled Model Intercomparison Project Phase 5 coupled climate models. In both models and observations, the seasonal heat budget is dominated by a local balance between net surface heating and storage in the heat content of the ocean and in melting/freezing of sea ice. Observations suggest ocean heat storage is more important than sea ice melt, while in most of these models, sea ice melt dominates. Seasonal horizontal heat flux divergence driven by the seasonal cycle of volume transport is only important locally. In models and observations, the dominant terms in the basin-average seasonal freshwater budget are the storages of freshwater between the ocean and sea ice, and the exchange between the two. The largest external source term is continental discharge in early summer, which is an order of magnitude smaller. The appearance of sea ice (extent and volume) and also ocean stratification in both the heat and freshwater budgets provides two links between the budgets and provides two mechanisms for feedback. One consequence of such an interaction is the fact that models with strong/weak seasonal surface heating also have strong/weak seasonal haline and temperature stratification.
C1 [Ding, Yanni; Carton, James A.; Chepurin, Gennady A.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Steele, Michael] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.
[Hakkinen, Sirpa] NOAA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Carton, JA (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
EM carton@atmos.umd.edu
FU National Science Foundation [OCE1233942]; NSF [OCE1233255]; Forum for
Arctic Modeling and Observational Synthesis (FAMOS)
FX Y.D., G.A.C., and J.A.C. gratefully acknowledge support from the
National Science Foundation (OCE1233942). Support for M.S. was provided
by NSF grant OCE1233255. We thank the World Climate Research Program's
Working Group on Coupled Modeling, which is responsible for CMIP, and
the climate modeling groups for producing and making available their
model output. For CMIP, the U.S. Department of Energy's Program for
Climate Model Diagnosis and Intercomparison (www-pcmdi.llnl.gov)
provides coordinating support and led development of software
infrastructure in partnership with the Global Organization for Earth
System Science Portals. We thank the Geophysical Fluid Dynamics
Laboratory for providing output from the two GFDL-ESM models used here.
We thank the ECMWF, NSIDC, and PSC teams for the ERA-40 atmospheric
fluxes, sea ice extent, PHC3.0 ocean climatology, and PIOMAS sea ice
volume data. ERA-40 data were downloaded from
http://apps.ecmwf.int/datasets/data/era40-moda/in 2014. The sea ice
extent was downloaded from http://nsidc.org/data/on February 2014. The
PHC3.0 ocean climatology was downloaded from
http://psc.apl.washington.edu/nonwp_projects/PHC/ on October 2013. The
PIOMAS data were downloaded from
http://psc.apl.uw.edu/research/projects/arctic-sea-ice-volume-anomaly/da
ta/on May 2015. We thank the support from Forum for Arctic Modeling and
Observational Synthesis (FAMOS).
NR 42
TC 1
Z9 1
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD APR
PY 2016
VL 121
IS 4
BP 2043
EP 2057
DI 10.1002/2015JC011124
PG 15
WC Oceanography
SC Oceanography
GA DW2HA
UT WOS:000383462300001
ER
PT J
AU Furst, S
Dow, T
Garrard, K
Sohn, A
Fixsen, D
Rinehart, S
Mentzell, E
Veach, T
Rizzo, M
Dhabal, A
AF Furst, Stephen
Dow, Tom
Garrard, Ken
Sohn, Alex
Fixsen, Dale
Rinehart, Stephen
Mentzell, Eric
Veach, Todd
Rizzo, Maxime
Dhabal, Arnab
TI Design and validation of the mounting structure for BETTII balloon-based
telescope with thin-walled optics
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE light-weight optics; diamond turning optics; optical mounting; kinematic
coupling; Balloon Experimental Twin Telescope for Infrared
Interferometry
ID INTERFEROMETRY; RESOLUTION
AB The NASA Balloon Experimental Twin Telescope for Infrared Interferometry (BETTII) system is designed to study the infrared emissions from star formation and active galactic nuclei through a double-Fourier Michelson interferometer located on a balloon at an altitude of 37 km. The BETTII external optics include a pair of identical beam-reducing, four-mirror telescopes, each with a 522-mm aperture, nonrotationally symmetric primary mirror. These telescopes were designed and assembled at the North Carolina State University Precision Engineering Consortium and are composed entirely of thin-walled aluminum components. The mounting structure is designed to be light weight and stiff to reduce thermal equilibration time in the rarified air at the edge of space and to maintain robust alignment of the optical elements. The mounts also prevent deformation of the large optical elements via custom-built kinematic Kelvin couplings and fixed-load clamps; the maximum form error of the optical surfaces are 300 nm RMS. This work details the design of the thin mirrors and mounting structure as well as validation of the mount assembly process, mount stiffness, and the kinematic couplings. (C) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Furst, Stephen; Dow, Tom; Garrard, Ken] North Carolina State Univ, Precis Engn Consortium, 1001 Capabil Dr, Raleigh, NC 27606 USA.
[Furst, Stephen] Smart Mat Solut Inc, 4713 Altha St, Raleigh, NC 27606 USA.
[Sohn, Alex] Oculus Res, 8747 148th Ave NE, Redmond, WA 98052 USA.
[Fixsen, Dale; Rinehart, Stephen; Mentzell, Eric; Veach, Todd; Rizzo, Maxime; Dhabal, Arnab] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Furst, S (reprint author), North Carolina State Univ, Precis Engn Consortium, 1001 Capabil Dr, Raleigh, NC 27606 USA.; Furst, S (reprint author), Smart Mat Solut Inc, 4713 Altha St, Raleigh, NC 27606 USA.
EM sjfurst@ncsu.edu
NR 13
TC 0
Z9 0
U1 0
U2 0
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD APR
PY 2016
VL 2
IS 2
AR 024001
DI 10.1117/1.JATIS.2.2.024001
PG 10
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DV7OV
UT WOS:000383126900001
ER
PT J
AU Sirbu, D
Thomas, SJ
Belikov, R
Lozi, J
Bendek, E
Pluzhnik, E
Lynch, DH
Hix, T
Zell, P
Guyon, O
Schneider, G
AF Sirbu, Dan
Thomas, Sandrine J.
Belikov, Ruslan
Lozi, Julien
Bendek, Eduardo
Pluzhnik, Eugene
Lynch, Dana H.
Hix, Troy
Zell, Peter
Guyon, Olivier
Schneider, Glenn
TI Demonstration of broadband contrast at 1.2 lambda/D and greater for the
EXCEDE starlight suppression system
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE high-contrast imaging; phase-induced amplitude apodization; coronagraph;
broadband; circumstellar debris systems; exoplanets; inner working
angle; EXoplanetary Circumstellar Environments and Disk Explorer
ID INDUCED AMPLITUDE APODIZATION; PHASE; CORONAGRAPH; ALGORITHM; PRINCIPLE
AB The EXoplanetary Circumstellar Environments and Disk Explorer (EXCEDE) science mission concept uses a visible-wavelength phase-induced amplitude apodization (PIAA) coronagraph to enable high-contrast imaging of circumstellar debris systems and some giant planets at angular separations reaching into the habitable zones of some of the nearest stars. We report on the experimental results obtained in the vacuum chamber at the Lockheed Martin Advanced Technology Center in 10% broadband light centered about 650 nm, with a median contrast of 1 x 10(-5) between 1.2 and 2.0 lambda/D simultaneously with 3 x 10(-7) contrast between 2 and 11 lambda/D for a single-sided dark hole using a deformable mirror (DM) upstream of the PIAA coronagraph. These results are stable and repeatable as demonstrated by three measurement runs with DM settings set from scratch and maintained on the best 90% out of the 1000 collected frames. We compare the reduced experimental data with simulation results from modeling observed experimental limits. The observed performance is consistent with uncorrected low-order modes not estimated by the low-order wavefront sensor. Modeled sensitivity to bandwidth and residual tip/tilt modes is well matched to the experiment. (C) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Sirbu, Dan; Belikov, Ruslan; Bendek, Eduardo; Pluzhnik, Eugene; Lynch, Dana H.; Zell, Peter] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Thomas, Sandrine J.] Large Synopt Survey Telescope, Tucson, AZ 85719 USA.
[Lozi, Julien; Guyon, Olivier] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Hix, Troy] Lockheed Martin Space Syst Co, Palo Alto, CA 94304 USA.
[Guyon, Olivier; Schneider, Glenn] Univ Arizona, Tucson, AZ 85721 USA.
RP Sirbu, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.; Schneider, G (reprint author), Univ Arizona, Tucson, AZ 85721 USA.
EM dan.sirbu@nasa.gov; gschneid@email.arizona.edu
NR 34
TC 0
Z9 0
U1 1
U2 1
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD APR
PY 2016
VL 2
IS 2
AR 025002
DI 10.1117/1.JATIS.2.2.025002
PG 14
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA DV7OV
UT WOS:000383126900003
ER
PT J
AU Melnyk, I
Matthews, B
Valizadegan, H
Banerjee, A
Oza, N
AF Melnyk, Igor
Matthews, Bryan
Valizadegan, Hamed
Banerjee, Arindam
Oza, Nikunj
TI Vector Autoregressive Model-Based Anomaly Detection in Aviation Systems
SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS
LA English
DT Article
ID TIME-SERIES; ALGORITHMS; SEQUENCES; SAFETY
AB Detecting anomalies in datasets, where each data object is a multivariate time series, possibly of different length for each data object, is emerging as a key problem in certain domains. The problem is considered in the context of aviation safety, where data objects are flights of various durations and the multivariate time series corresponds to sensor readings. The goal is then to detect anomalous flight segments, due to mechanical, environmental, or human factors. In this paper, a general framework is presented for anomaly detection in such settings by representing each multivariate time series using a vector autoregressive exogenous model, constructing a distance matrix among the objects based on their respective vector autoregressive exogenous models, and finally detecting anomalies based on the object dissimilarities. The framework is scalable, due to the inherent parallel nature of most computations, and can be used to perform online anomaly detection. Experimental results on a real flight dataset illustrate that the framework can detect different types of multivariate anomalies along with the key parameters involved.
C1 [Melnyk, Igor; Banerjee, Arindam] Univ Minnesota, Dept Comp Sci & Engn, Minneapolis, MN 55455 USA.
[Matthews, Bryan; Valizadegan, Hamed; Oza, Nikunj] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Matthews, Bryan] Stinger Ghaffarian Technol Inc, Greenbelt, MD USA.
RP Melnyk, I (reprint author), Univ Minnesota, Dept Comp Sci & Engn, Minneapolis, MN 55455 USA.
FU NASA [NNX12AQ39A]; National Science Foundation [IIS-1447566,
IIS-1422557, CCF-1451986, CNS-1314560, IIS-0953274, IIS-1029711]
FX The research was supported by NASA Cooperative Agreement NNX12AQ39A and
National Science Foundation grants IIS-1447566, IIS-1422557,
CCF-1451986, CNS-1314560, IIS-0953274, and IIS-1029711.
NR 40
TC 0
Z9 0
U1 1
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 1940-3151
EI 2327-3097
J9 J AEROSP INFORM SYST
JI J. Aerosp. Inf. Syst.
PD APR
PY 2016
VL 13
IS 4
BP 161
EP 173
DI 10.2514/1.I010394
PG 13
WC Engineering, Aerospace
SC Engineering
GA DU9DW
UT WOS:000382517500002
ER
PT J
AU Andren, M
Stockmann, G
Skelton, A
Sturkell, E
Morth, CM
Gudrunardottir, HR
Keller, NS
Odling, N
Dahren, B
Broman, C
Balic-Zunic, T
Hjartarson, H
Siegmund, H
Freund, F
Kockum, I
AF Andren, Margareta
Stockmann, Gabrielle
Skelton, Alasdair
Sturkell, Erik
Morth, Carl-Magnus
Gudrunardottir, Helga Rakel
Keller, Nicole Simone
Odling, Nic
Dahren, Borje
Broman, Curt
Balic-Zunic, Tonci
Hjartarson, Hreinn
Siegmund, Heike
Freund, Friedemann
Kockum, Ingrid
TI Coupling between mineral reactions, chemical changes in groundwater, and
earthquakes in Iceland
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID REPLACEMENT REACTIONS; RAMAN-SPECTROSCOPY; KOBE EARTHQUAKE; PRECURSORS;
PREDICTION; WATER; MECHANISMS; ANALCIME; SPRINGS; GROWTH
AB Chemical analysis of groundwater samples collected from a borehole at Hafralaekur, northern Iceland, from October 2008 to June 2015 revealed (1) a long-term decrease in concentration of Si and Na and (2) an abrupt increase in concentration of Na before each of two consecutive M 5 earthquakes which occurred in 2012 and 2013, both 76km from Hafralaekur. Based on a geochemical (major elements and stable isotopes), petrological, and mineralogical study of drill cuttings taken from an adjacent borehole, we are able to show that (1) the long-term decrease in concentration of Si and Na was caused by constant volume replacement of labradorite by analcime coupled with precipitation of zeolites in vesicles and along fractures and (2) the abrupt increase of Na concentration before the first earthquake records a switchover to nonstoichiometric dissolution of analcime with preferential release of Na into groundwater. We attribute decay of the Na peaks, which followed and coincided with each earthquake to uptake of Na along fractured or porous boundaries between labradorite and analcime crystals. Possible causes of these Na peaks are an increase of reactive surface area caused by fracturing or a shift from chemical equilibrium caused by mixing between groundwater components. Both could have been triggered by preseismic dilation, which was also inferred in a previous study by Skelton et al. (2014). The mechanism behind preseismic dilation so far from the focus of an earthquake remains unknown.
C1 [Andren, Margareta; Stockmann, Gabrielle; Skelton, Alasdair; Morth, Carl-Magnus; Gudrunardottir, Helga Rakel; Broman, Curt; Siegmund, Heike] Stockholm Univ, Dept Geol Sci, Stockholm, Sweden.
[Sturkell, Erik] Univ Gothenburg, Dept Earth Sci, Gothenburg, Sweden.
[Keller, Nicole Simone] Univ Iceland, Inst Earth Sci, Reykjavik, Iceland.
[Odling, Nic] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland.
[Dahren, Borje] Uppsala Univ, Dept Earth Sci, Uppsala, Sweden.
[Balic-Zunic, Tonci] Univ Copenhagen, Nat Hist Museum, Copenhagen, Denmark.
[Hjartarson, Hreinn] Landsvirkjun, Reykjavik, Iceland.
[Freund, Friedemann] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
[Kockum, Ingrid] Karolinska Inst, Stockholm, Sweden.
RP Stockmann, G (reprint author), Stockholm Univ, Dept Geol Sci, Stockholm, Sweden.
EM gabrielle.stockmann@geo.su.se
OI Dahren, Borje/0000-0002-9274-6998
FU Swedish Research Council
FX We would like to thank the reviewers Steve Ingebritsen and Monica Piochi
for their valuable comments, which greatly improved the manuscript. Our
most sincere thanks go to Berndt Nyberg for assistance during fieldwork
and general support. Dan Zetterberg is thanked for sample preparation at
Stockholm University. The Icelandic Metrological Office is thanked for
the earthquake data. Financial support from the Swedish Research Council
is gratefully acknowledged. All data are available from Alasdair
Skelton, Stockholm University (Alasdair.Skelton@geo.su.se).
NR 48
TC 1
Z9 1
U1 10
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD APR
PY 2016
VL 121
IS 4
BP 2315
EP 2337
DI 10.1002/2015JB012614
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DT6WY
UT WOS:000381626700007
ER
PT J
AU Adhikari, S
Ivins, ER
AF Adhikari, Surendra
Ivins, Erik R.
TI Climate-driven polar motion: 2003-2015
SO SCIENCE ADVANCES
LA English
DT Article
ID GLACIAL ISOSTATIC-ADJUSTMENT; SEA-LEVEL; EARTH ROTATION; RECONCILED
ESTIMATE; ICE-SHEET; GRACE; ANTARCTICA; MODEL
AB Earth's spin axis has been wandering along the Greenwich meridian since about 2000, representing a 75 degrees eastward shift from its long-term drift direction. The past 115 years have seen unequivocal evidence for a quasi-decadal periodicity, and these motions persist throughout the recent record of pole position, in spite of the new drift direction. We analyze space geodetic and satellite gravimetric data for the period 2003-2015 to show that all of the main features of polar motion are explained by global-scale continent-ocean mass transport. The changes in terrestrial water storage (TWS) and global cryosphere together explain nearly the entire amplitude (83 +/- 23%) and mean directional shift (within 5.9 degrees +/- 7.6 degrees) of the observed motion. We also find that the TWS variability fully explains the decadal-like changes in polar motion observed during the study period, thus offering a clue to resolving the long-standing quest for determining the origins of decadal oscillations. This newly discovered link between polar motion and global-scale TWS variability has broad implications for the study of past and future climate.
C1 [Adhikari, Surendra; Ivins, Erik R.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Adhikari, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM surendra.adhikari@jpl.nasa.gov
RI Ivins, Erik/C-2416-2011
NR 50
TC 8
Z9 8
U1 4
U2 5
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 2375-2548
J9 SCI ADV
JI Sci. Adv.
PD APR
PY 2016
VL 2
IS 4
AR e1501693
DI 10.1126/sciadv.1501693
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DR7IB
UT WOS:000380072100032
PM 27152348
ER
PT J
AU England, SL
Liu, GP
Withers, P
Yigit, E
Lo, D
Jain, S
Schneider, NM
Deighan, J
McClintock, WE
Mahaffy, PR
Elrod, M
Benna, M
Jakosky, BM
AF England, Scott L.
Liu, Guiping
Withers, Paul
Yigit, Erdal
Lo, Daniel
Jain, Sonal
Schneider, Nicholas M.
Deighan, Justin
McClintock, William E.
Mahaffy, Paul R.
Elrod, Meredith
Benna, Mehdi
Jakosky, Bruce M.
TI Simultaneous observations of atmospheric tides from combined in situ and
remote observations at Mars from the MAVEN spacecraft
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID NONMIGRATING TIDES; MARTIAN ATMOSPHERE; MGS ACCELEROMETER; GLOBAL
SURVEYOR; THERMAL TIDES; CO CAMERON; DAYGLOW
AB We report the observations of longitudinal variations in the Martian thermosphere associated with nonmigrating tides. Using the Neutral Gas Ion Mass Spectrometer (NGIMS) and the Imaging Ultraviolet Spectrograph (IUVS) on NASA's Mars Atmosphere and Volatile EvolutioN Mission (MAVEN) spacecraft, this study presents the first combined analysis of in situ and remote observations of atmospheric tides at Mars for overlapping volumes, local times, and overlapping date ranges. From the IUVS observations, we determine the altitude and latitudinal variation of the amplitude of the nonmigrating tidal signatures, which is combined with the NGIMS, providing information on the compositional impact of these waves. Both the observations of airglow from IUVS and the CO2 density observations from NGIMS reveal a strong wave number 2 signature in a fixed local time frame. The IUVS observations reveal a strong latitudinal dependence in the amplitude of the wave number 2 signature. Combining this with the accurate CO2 density observations from NGIMS, this would suggest that the CO2 density variation is as high as 27% at 0-10 degrees latitude. The IUVS observations reveal little altitudinal dependence in the amplitude of the wave number 2 signature, varying by only 20% from160 to 200 km. Observations of five different species with NGIMS show that the amplitude of the wave number 2 signature varies in proportion to the inverse of the species scale height, giving rise to variation in composition as a function of longitude. The analysis and discussion here provide a roadmap for further analysis as additional coincident data from these two instruments become available.
C1 [England, Scott L.; Liu, Guiping] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Withers, Paul] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Yigit, Erdal] George Mason Univ, Space Weather Lab, Dept Phys & Astron, Fairfax, VA 22030 USA.
[Lo, Daniel] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Jain, Sonal; Schneider, Nicholas M.; Deighan, Justin; McClintock, William E.; Jakosky, Bruce M.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Mahaffy, Paul R.; Elrod, Meredith; Benna, Mehdi] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP England, SL (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM england@ssl.berkeley.edu
RI Yigit, Erdal/C-8609-2009;
OI Yigit, Erdal/0000-0002-2819-2521; SCHNEIDER,
NICHOLAS/0000-0001-6720-5519
FU NASA [NNX13AO36G, NNX13AO35G]
FX All data used in the study are archived in the Planetary Atmospheres
Node of the Planetary Data System (http://pds.nasa.gov). S.L.E., G.L.,
and E.Y. were supported by NASA grant NNX13AO36G. P.W. was supported by
NASA grant NNX13AO35G. The MAVEN mission has been funded by NASA through
the Mars Exploration Program.
NR 35
TC 3
Z9 3
U1 4
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR
PY 2016
VL 121
IS 4
BP 594
EP 607
DI 10.1002/2016JE004997
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DR5EZ
UT WOS:000379927400003
ER
PT J
AU Turner, SMR
Bridges, JC
Grebby, S
Ehlmann, BL
AF Turner, Stuart M. R.
Bridges, John C.
Grebby, Stephen
Ehlmann, Bethany L.
TI Hydrothermal activity recorded in post Noachian-aged impact craters on
Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID NAKHLITE MARTIAN METEORITES; ORBITAL IDENTIFICATION; MINERAL
ASSEMBLAGES; AQUEOUS ALTERATION; HYDROUS MINERALS; CLAY FORMATION;
SPECTROSCOPY; REFLECTANCE; PHYLLOSILICATES; SMECTITES
AB Hydrothermal systems have previously been reported in ancient Noachian and Hesperian-aged craters on Mars using CRISM but not in Amazonian-aged impact craters. However, the nakhlite meteorites do provide evidence of Amazonian hydrothermal activity. This study uses CRISM data of 144 impact craters of >= 7 km diameter and 14 smaller craters (3-7 km diameter) within terrain mapped as Amazonian to search for minerals that may have formed as a result of impact-induced hydrothermal alteration or show excavation of ancient altered crust. No evidence indicating the presence of hydrated minerals was found in the 3-7km impact craters. Hydrated minerals were identified in three complex impact craters, located at 52.42 degrees N, 39.86 degrees E in the Ismenius Lacus quadrangle, at 8.93 degrees N, 141.28 degrees E in Elysium, and within the previously studied Stokes crater. These three craters have diameters 20 km, 62 km, and 51 km. The locations of the hydrated mineral outcrops and their associated morphology indicate that two (o)f these three impact craters-the unnamed Ismenius Lacus Crater and Stokes Crater-possibly hosted impact-induced hydrothermal systems, as they contain alteration assemblages on their central uplifts that are not apparent in their ejecta. Chlorite and Fe serpentine are identified within alluvial fans in the central uplift and rim of the Ismenius Lacus crater, whereas Stokes crater contains a host of Fe/Mg/Al phyllosilicates. However, excavation origin cannot be precluded. Our work suggests that impact-induced hydrothermalism was rare in the Amazonian and/or that impact-induced hydrothermal alteration was not sufficiently pervasive or spatially widespread for detection by CRISM.
C1 [Turner, Stuart M. R.; Bridges, John C.] Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester, Leics, England.
[Grebby, Stephen] British Geol Survey, Nottingham, England.
[Ehlmann, Bethany L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Bridges, JC (reprint author), Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester, Leics, England.
EM j.bridges@leicester.ac.uk
RI BGS University Funding Initiative, BUFI/H-4822-2011;
OI BGS University Funding Initiative, BUFI/0000-0003-3097-5530; Grebby,
Stephen/0000-0001-9768-2682
FU joint STFC-NERC (British Geological Survey) CASE studentship
FX Turner was funded by a joint STFC-NERC (British Geological Survey) CASE
studentship. Grebby publishes with the permission of the Executive
Director, British Geological Survey (NERC). We would like to thank MRO
and MOLA science teams for their work in acquiring and processing the
data. CRISM data used in this paper are available from the NASA
Planetary Data System Geoscience Node
(http://pds-geosciences.wustl.edu/missions/mro/crism.htm), HiRISE images
are available from the University of Arizona HiRISE website
(https://hirise.lpl.arizona.edu/), CTX images are available from the
Image Explorer on the Arizona State University website
(http://viewer.mars.asu.edu/viewer/ctx#T=0), and MOLA data are available
from the United States Geological Survey Planetary GIS Web Server
(http://webgis.wr.usgs.gov/pigwad/down/mars_dl.htm). We thank Cong Pan
and an anonymous reviewer for their comments.
NR 76
TC 0
Z9 0
U1 3
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR
PY 2016
VL 121
IS 4
BP 608
EP 625
DI 10.1002/2015JE004989
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DR5EZ
UT WOS:000379927400004
ER
PT J
AU Zent, AP
Hecht, MH
Hudson, TL
Wood, SE
Chevrier, VF
AF Zent, A. P.
Hecht, M. H.
Hudson, T. L.
Wood, S. E.
Chevrier, V. F.
TI A revised calibration function and results for the Phoenix mission TECP
relative humidity sensor
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MARS WATER-VAPOR; VERTICAL-DISTRIBUTION; LANDING SITE; ICE; H2O
AB A new calibration function for the humidity sensor in the Thermal and Electrical Conductivity Probe (TECP) on the Phoenix (PHX) Mars mission has been developed. Two changes are incorporated: (1) it is now cast in terms of frost point (T-f) rather than relative humidity (RH), and (2) flight data, taken when the atmosphere is independently known to be saturated, are included in the calibration data set. Daytime (6: 00 h-19: 00 h) frost points ranged from 194 K to 209 K; the nighttime frost point ranged from 179 K to 206 K. The response of the sensor was smooth and continuous throughout. Daytime humidity exhibited large, high-frequency variance driven by turbulence, whereas nighttime humidity varied smoothly with the temperature of the atmosphere. Nighttime saturation of the atmosphere begins at L-s 101 degrees, (Martian solar day (sol) 55), which is earlier than reported by either Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) or solid-state imager (SSI). Early mornings are the most humid part of the sol after L-s 113 degrees (sol 80), due to sublimation of surface ice that precipitates overnight. H2O is removed from the atmosphere into the regolith, mostly during the late afternoon, although this continues into the evening. The ground ice exposed by Phoenix operations masks the naturally occurring process in the early evening and may cause the atmosphere immediately around the lander to saturate somewhat earlier in the evening than it otherwise would have. The average H2O vapor density is close to the summertime value expected for equilibrium with ground ice. A discrepancy between the H2O column calculated from TECP data and the column measured by CRISM and SSI is likely due to comparable timescales between turbulent mixing through the planetary boundary layer and adsorptive drawdown of H2O. We find that RH is mostly < 5% (daytime) or > 95% (nighttime), and the transition between the two extremes is extremely rapid.
C1 [Zent, A. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hecht, M. H.] MIT Haystack Observ, Westford, MA USA.
[Hudson, T. L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Wood, S. E.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Chevrier, V. F.] Univ Arkansas, Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA.
RP Zent, AP (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Aaron.P.Zent@nasa.gov
RI Wood, Stephen/R-5592-2016
OI Wood, Stephen/0000-0002-9330-434X
FU Mars Data Analysis Program
FX The authors would like to thank Bob Haberle, Leslie Tamppari, and
Christine Hostein-Rathlou for helpful discussions. The research was
supported through the Mars Data Analysis Program. All data used in this
paper are available at the vi Planetary Data System. TECP data is found
at
http://pds-geosciences.wustl.edu/phx/phx-m-meca-2-niedr-v1/phxmec_0xxx/.
MET data are found at:
http://pds-atmospheres.nmsu.edu/pdsd/archive/data/phx-m-met-3-pt-rdr-v10
/
NR 53
TC 0
Z9 0
U1 2
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR
PY 2016
VL 121
IS 4
BP 626
EP 651
DI 10.1002/2015JE004933
PG 26
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DR5EZ
UT WOS:000379927400005
ER
PT J
AU Lillis, RJ
Lee, CO
Larson, D
Luhmann, JG
Halekas, JS
Connerney, JEP
Jakosky, BM
AF Lillis, Robert J.
Lee, Christina O.
Larson, Davin
Luhmann, Janet G.
Halekas, Jasper S.
Connerney, Jack E. P.
Jakosky, Bruce M.
TI Shadowing and anisotropy of solar energetic ions at Mars measured by
MAVEN during the March 2015 solar storm
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID PARTICLE; ENVIRONMENT; IONOSPHERE; PHOBOS-2; MODEL
AB The Solar Energetic Particle (SEP) Instrument on the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft is meant to characterize the variability of SEP fluxes at Mars. SEP ion precipitation is an important source of heating, ionization, and chemical changes in the upper atmosphere of Mars and may have played a substantial role in driving atmospheric escape over the history of the solar system. Here we examine SEP fluxes during a series of solar disturbances in late February through early March 2015. We present the first SEP ion pitch angle distributions measured at Mars and show how SEP anisotropy changes over the course of the event period. We present examples and explanations of several different kinds of variability in the SEP flux measured in the four fields of view of the instrument. Finally, we present a statistical study of energy-and angle-dependent shadowing of SEP under three different sets of heliospheric conditions, showing that the direct shadowing of SEP by the solid planet may be better explained in terms of simple geometry under quieter heliospheric conditions. In-depth understanding of the effects on SEP fluxes and precipitation patterns by the complex interplay between solar wind disturbances and Mars' magnetospheric configuration awaits detailed modeling studies.
C1 [Lillis, Robert J.; Lee, Christina O.; Larson, Davin; Luhmann, Janet G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Halekas, Jasper S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Connerney, Jack E. P.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Jakosky, Bruce M.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Lillis, RJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM rlillis@SSL.Berkeley.edu
OI Lee, Christina/0000-0002-1604-3326; connerney, jack/0000-0001-7478-6462
NR 27
TC 0
Z9 0
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2016
VL 121
IS 4
BP 2818
EP 2829
DI 10.1002/2015JA022327
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DR5RO
UT WOS:000379960300001
ER
PT J
AU Boardsen, SA
Hospodarsky, GB
Kletzing, CA
Engebretson, MJ
Pfaff, RF
Wygant, JR
Kurth, WS
Averkamp, TF
Bounds, SR
Green, JL
De Pascuale, S
AF Boardsen, Scott A.
Hospodarsky, George B.
Kletzing, Craig A.
Engebretson, Mark J.
Pfaff, Robert F.
Wygant, John R.
Kurth, William S.
Averkamp, Terrance F.
Bounds, Scott R.
Green, Jim L.
De Pascuale, Sebastian
TI Survey of the frequency dependent latitudinal distribution of the fast
magnetosonic wave mode from Van Allen Probes Electric and Magnetic Field
Instrument and Integrated Science waveform receiver plasma wave analysis
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EQUATORIAL NOISE EMISSIONS; CLUSTER SPACECRAFT; RING DISTRIBUTIONS;
ENERGETIC IONS; PROTON; MAGNETOSPHERE; INSTABILITY; EXCITATION
AB We present a statistical survey of the latitudinal structure of the fast magnetosonic wave mode detected by the Van Allen Probes spanning the time interval of 21 September 2012 to 1 August 2014. We show that statistically, the latitudinal occurrence of the wave frequency (f) normalized by the local proton cyclotron frequency (f(cP)) has a distinct funnel-shaped appearance in latitude about the magnetic equator similar to that found in case studies. By comparing the observed E/B ratios with the model E/B ratio, using the observed plasma density and background magnetic field magnitude as input to the model E/B ratio, we show that this mode is consistent with the extra-ordinary (whistler) mode at wave normal angles (theta(k)) near 90 degrees. Performing polarization analysis on synthetic waveforms composed from a superposition of extra-ordinary mode plane waves with theta(k) randomly chosen between 87 and 90 degrees, we show that the uncertainty in the derived wave normal is substantially broadened, with a tail extending down to theta(k) of 60 degrees, suggesting that another approach is necessary to estimate the true distribution of theta(k). We find that the histograms of the synthetically derived ellipticities and theta(k) are consistent with the observations of ellipticities and theta(k) derived using polarization analysis. We make estimates of the median equatorial theta(k) by comparing observed and model ray tracing frequency-dependent probability occurrence with latitude and give preliminary frequency dependent estimates of the equatorial theta(k) distribution around noon and 4 R-E, with the median of similar to 4 to 7 degrees from 90 degrees at f/f(cP) = 2 and dropping to similar to 0.5 degrees from 90 degrees at f/f(cP) = 30. The occurrence of waves in this mode peaks around noon near the equator at all radial distances, and we find that the overall intensity of these waves increases with AE*, similar to findings of other studies.
C1 [Boardsen, Scott A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Boardsen, Scott A.; Pfaff, Robert F.] NASA GSFC, Greenbelt, MD USA.
[Hospodarsky, George B.; Kletzing, Craig A.; Kurth, William S.; Averkamp, Terrance F.; Bounds, Scott R.; De Pascuale, Sebastian] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Engebretson, Mark J.] Augsburg Coll, Dept Phys, Minneapolis, MN USA.
[Wygant, John R.] Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA.
[Green, Jim L.] NASA Headquarters, Planetary Sci Div, Washington, DC USA.
RP Boardsen, SA (reprint author), Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.; Boardsen, SA (reprint author), NASA GSFC, Greenbelt, MD USA.
EM Scott.A.Boardsen@nasa.gov
OI De Pascuale, Sebastian/0000-0001-7142-0246
FU NASA [NAS5-01072]; JHU/APL [921647]
FX We thank Dr. K. Ronnmark at Umea University in Sweden for providing us
with the warm plasma instability code WHAMP. The EMFISIS data can be
obtained from the electronic archive at the Space Physics Data Facility
(http://spdf.gsfc.nasa.gov/). We acknowledge use of NASA/GSFC's Space
Physics Data Facility's OMNIWeb (or CDAWeb or ftp) service and OMNI
data. The EFW-derived densities, from potentials, are available at
http://www.space.umn.edu/rbspefw-data. The shadow times of the
antisunward short antenna are available at
http://emfisis.physics.uiowa.edu/events/rbsp-a/SP5antinshadow/ and
http://emfisis.physics.uiowa.edu/events/rbsp-b/SP5antinshadow/. The
EMFISIS-WFR noise levels are available at
http://emfisis.physics.uiowa.edu/events/rbsp-a/backgrounds/ and
http://emfisis.physics.uiowa.edu/events/rbsp-b/backgrounds/. At Goddard
this study was supported by NASA prime contract NAS5-01072. The research
at The University of Iowa was supported by JHU/APL contract 921647 under
NASA Prime contract NAS5-01072.
NR 46
TC 8
Z9 8
U1 3
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2016
VL 121
IS 4
BP 2902
EP 2921
DI 10.1002/2015JA021844
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DR5RO
UT WOS:000379960300007
ER
PT J
AU Masunaga, K
Seki, K
Brain, DA
Fang, X
Dong, Y
Jakosky, BM
McFadden, JP
Halekas, JS
Connerney, JEP
AF Masunaga, K.
Seki, K.
Brain, D. A.
Fang, X.
Dong, Y.
Jakosky, B. M.
McFadden, J. P.
Halekas, J. S.
Connerney, J. E. P.
TI O+ ion beams reflected below the Martian bow shock: MAVEN observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MAGNETIC PILEUP BOUNDARY; SOLAR-WIND INTERACTION; PICKUP IONS; PHOBOS
OBSERVATIONS; MARS; ATMOSPHERE; VENUS; PRECIPITATION; ENVIRONMENT;
PLANETS
AB We investigate a generation mechanism of O+ ion beams observed above the Martian bow shock by analyzing ion velocity distribution functions (VDFs) measured by the Suprathermal and Thermal Ion Composition instrument on the Mars Atmosphere and Volatile Evolution (MAVEN) spacecraft. In the solar wind near Mars, MAVEN often observes energetic O+ ion beams (similar to 10 keV or higher). Accompanied with the O+ ion beam events, we sometimes observe characteristic ion VDFs in the magnetosheath: a partial ring distribution. The partial ring distribution corresponds to pickup ions with a finite initial velocity (i.e., not newborn pickup ions), and its phase space density is much smaller than that of local pickup O+ ions of the magnetosheath. Thus, the partial ring distribution is most likely produced by the reflection of pickup O+ ions precipitating from the upstream solar wind below the bow shock. After being injected into the magnetosheath from the solar wind, the precipitating O+ ions are subject to the significantly enhanced magnetic field in this region and start to gyrate around the guiding center of the plasma frame in the magnetosheath. Consequently, a part of precipitating O+ ions are reflected back to the solar wind, generating O+ beams in the solar wind. The beams direct quasi-sunward near the subsolar region but have large angle with respect to the sunward direction at high solar zenith angles (>50 degrees). The reflected O+ beams are accelerated by the convection electric field of the solar wind and may escape Mars.
C1 [Masunaga, K.; Seki, K.] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Tokyo, Japan.
[Brain, D. A.; Fang, X.; Dong, Y.; Jakosky, B. M.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[McFadden, J. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Halekas, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Connerney, J. E. P.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Masunaga, K (reprint author), Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Tokyo, Japan.
EM masu-kei@eps.s.u-tokyo.ac.jp
RI Fang, Xiaohua/C-2773-2008
OI Fang, Xiaohua/0000-0002-6584-2837
FU Program for Advancing Strategic International Networks to Accelerate the
Circulation of Talented Researchers from JSPS [G2602]; MEXT of Japan;
JSPS [14J03613]; NASA through the Mars Exploration Program; [15H0731]
FX This work was supported by Grant-in-Aid for Scientific Research (B)
15H0731 and by the Program for Advancing Strategic International
Networks to Accelerate the Circulation of Talented Researchers G2602
from JSPS and MEXT of Japan. This work was also supported by
Grant-in-Aid for JSPS Fellows 14J03613 from JSPS. The MAVEN project is
supported by NASA through the Mars Exploration Program. The MAVEN data
are available in NASA Planetary Data System.
NR 42
TC 1
Z9 1
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2016
VL 121
IS 4
BP 3093
EP 3107
DI 10.1002/2016JA022465
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DR5RO
UT WOS:000379960300019
ER
PT J
AU Andrews, DJ
Barabash, S
Edberg, NJT
Gurnett, DA
Hall, BES
Holmstrom, M
Lester, M
Morgan, DD
Opgenoorth, HJ
Ramstad, R
Sanchez-Cano, B
Way, M
Witasse, O
AF Andrews, D. J.
Barabash, S.
Edberg, N. J. T.
Gurnett, D. A.
Hall, B. E. S.
Holmstrom, M.
Lester, M.
Morgan, D. D.
Opgenoorth, H. J.
Ramstad, R.
Sanchez-Cano, B.
Way, M.
Witasse, O.
TI Plasma observations during the Mars atmospheric "plume" event of
March-April 2012
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CORONAL MASS EJECTIONS; SOLAR-WIND; NUMERICAL-SIMULATION; MARTIAN
IONOSPHERE; CME EVENT; EXPRESS; ASPERA-3; SOUNDER; AURORA; DUST
AB We present initial analyses and conclusions from plasma observations made during the reported "Mars plume event" of March-April 2012. During this period, multiple independent amateur observers detected a localized, high-altitude "plume" over the Martian dawn terminator, the cause of which remains to be explained. The estimated brightness of the plume exceeds that expected for auroral emissions, and its projected altitude greatly exceeds that at which clouds are expected to form. We report on in situ measurements of ionospheric plasma density and solar wind parameters throughout this interval made by Mars Express, obtained over the same surface region but at the opposing terminator. Measurements in the ionosphere at the corresponding location frequently show a disturbed structure, though this is not atypical for such regions with intense crustal magnetic fields. We tentatively conclude that the formation and/or transport of this plume to the altitudes where it was observed could be due in part to the result of a large interplanetary coronal mass ejection (ICME) encountering the Martian system. Interestingly, we note that the only similar plume detection in May 1997 may also have been associated with a large ICME impact at Mars.
C1 [Andrews, D. J.; Edberg, N. J. T.; Opgenoorth, H. J.] Swedish Inst Space Phys, Uppsala, Sweden.
[Barabash, S.; Holmstrom, M.; Ramstad, R.] Swedish Inst Space Phys, Kiruna, Sweden.
[Gurnett, D. A.; Morgan, D. D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Hall, B. E. S.; Lester, M.; Sanchez-Cano, B.] Univ Leicester, Dept Phys & Astron, Leicester, Leics, England.
[Way, M.] NASA Goddard Inst Space Studies, New York, NY USA.
[Way, M.] Uppsala Univ, Dept Phys & Astron, Uppsala, Sweden.
[Witasse, O.] ESA ESTEC, Noordwijjk, Netherlands.
RP Andrews, DJ (reprint author), Swedish Inst Space Phys, Uppsala, Sweden.
EM david.andrews@irfu.se
RI Lester, Mark/C-9657-2016;
OI Lester, Mark/0000-0001-7353-5549; Holmstrom, Mats/0000-0001-5494-5374;
Way, Michael/0000-0003-3728-0475
FU Swedish National Space Board [DNR 162/14]; Swedish Research Council [DNR
621-2014-5526]; NASA from the Jet Propulsion Laboratory [1224107]; STFC
[ST/K001000/1, ST/K502121/1]; NASA's Science Mission Directorate
FX Work at IRF was supported by grants from the Swedish National Space
Board (DNR 162/14) and the Swedish Research Council (DNR 621-2014-5526).
Work at Iowa was supported by NASA through contract 1224107 from the Jet
Propulsion Laboratory. Work at Leicester was supported by STFC grants
ST/K001000/1 and ST/K502121/1. M.J.W.: The results reported herein
benefitted from participation in NASA's Nexus for Exoplanet System
Science (NExSS) research oordination network sponsored by NASA's Science
Mission Directorate. We thank A. Sanchez-Lavega for the provision of
summaries of raw data. We thank K.C. Hansen and B. Zieger for providing
solar wind propagations from their Michigan Solar Wind Model
(http://mswim.engin.umich.edu/). Finally, we thank both referees for
their helpful comments.
NR 53
TC 0
Z9 0
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2016
VL 121
IS 4
BP 3139
EP 3154
DI 10.1002/2015JA022023
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DR5RO
UT WOS:000379960300022
ER
PT J
AU Omidi, N
Berchem, J
Sibeck, D
Zhang, H
AF Omidi, N.
Berchem, J.
Sibeck, D.
Zhang, H.
TI Impacts of spontaneous hot flow anomalies on the magnetosheath and
magnetopause
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EARTHS BOW SHOCK; DIAMAGNETIC CAVITIES; CLUSTER OBSERVATIONS; FORESHOCK
CAVITONS; HYBRID SIMULATION; PLASMA STRUCTURES; DISCONTINUITY;
CONVECTION; GENERATION; JETS
AB Spacecraft observations and global hybrid (kinetic ions and fluid electrons) simulations have demonstrated that ion dissipation processes at the quasi-parallel bow shock are associated with the formation of structures called spontaneous hot flow anomalies (SHFAs). Previous simulations and recent spacecraft observations have also established that SHFAs result in the formation of magnetosheath filamentary structures (MFS). In this paper we demonstrate that in addition to MFS, SHFAs also result in the formation of magnetosheath cavities that are associated with decreases in density, velocity, and magnetic field and enhancements in temperature. We use the results of a global MHD run to determine the change in the magnetosheath properties associated with cavities due to ion kinetic effects. The results also show the formation of regions of high flow speed called magnetosheath jets whose properties as a function of solar wind Mach number are described in this study. Comparing the properties of the simulated magnetosheath cavities and jets to past spacecraft observations provides good agreement in both cases. We also demonstrate that pressure variations associated with cavities and SHFAs in the sheath result in a continuous sunward and antisunward magnetopause motion. This result is consistent with previous suggestions that SHFAs may be responsible for the generation of ion cyclotron waves and precipitation of ring current protons in the outer magnetosphere.
C1 [Omidi, N.] Solana Sci Inc, Solana Beach, CA 92075 USA.
[Berchem, J.] Univ Calif Los Angeles, IGPP, Los Angeles, CA USA.
[Sibeck, D.] NASA GSFC, Greenbelt, MD USA.
[Zhang, H.] Univ Alaska Fairbanks, Lab Extraterr Phys, Fairbanks, AK USA.
RP Omidi, N (reprint author), Solana Sci Inc, Solana Beach, CA 92075 USA.
EM omidi@solanasci.com
FU NSF [AGS-1007449, AGS-1103227, AGS-110326]; THEMIS mission
FX Work for this project was supported by NSF grants AGS-1007449 and
AGS-1103227. Work at UCLA was supported by NSF grant AGS-110326. Work at
GSFC was supported by the THEMIS mission. Request for simulation data
used in this study may be made to N. Omidi at omidi@solanasci.com.
NR 45
TC 1
Z9 1
U1 3
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2016
VL 121
IS 4
BP 3155
EP 3169
DI 10.1002/2015JA022170
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DR5RO
UT WOS:000379960300023
ER
PT J
AU Walsh, BM
Collier, MR
Kuntz, KD
Porter, FS
Sibeck, DG
Snowden, SL
Carter, JA
Collado-Vega, Y
Connor, HK
Cravens, TE
Read, AM
Sembay, S
Thomas, NE
AF Walsh, B. M.
Collier, M. R.
Kuntz, K. D.
Porter, F. S.
Sibeck, D. G.
Snowden, S. L.
Carter, J. A.
Collado-Vega, Y.
Connor, H. K.
Cravens, T. E.
Read, A. M.
Sembay, S.
Thomas, N. E.
TI Wide field-of-view soft X-ray imaging for solar wind-magnetosphere
interactions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID TRANSPOLAR POTENTIAL SATURATION; CHARGE-EXCHANGE EMISSION; ART. NO.
A09203; XMM-NEWTON; EARTHS MAGNETOPAUSE; MAGNETIC-FIELD; POLAR; CUSP;
DISCOVERY; CHANDRA
AB Soft X-ray imagers can be used to study the mesoscale and macroscale density structures that occur whenever and wherever the solar wind encounters neutral atoms at comets, the Moon, and both magnetized and unmagnetized planets. Charge exchange between high charge state solar wind ions and exospheric neutrals results in the isotropic emission of soft X-ray photons with energies from 0.1 to 2.0 keV. At Earth, this process occurs primarily within the magnetosheath and cusps. Through providing a global view, wide field-of-view imaging can determine the significance of the various proposed solar wind-magnetosphere interaction mechanisms by evaluating their global extent and occurrence patterns. A summary of wide field-of-view (several to tens of degrees) soft X-ray imaging is provided including slumped micropore microchannel reflectors, simulated images, and recent flight results.
C1 [Walsh, B. M.] Boston Univ, Dept Mech Engn & Ctr, Boston, MA 02215 USA.
[Collier, M. R.; Porter, F. S.; Sibeck, D. G.; Snowden, S. L.; Collado-Vega, Y.; Connor, H. K.; Thomas, N. E.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
[Carter, J. A.; Read, A. M.; Sembay, S.] Univ Leicester, Dept Phys & Astron, Leicester, Leics, England.
[Cravens, T. E.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
RP Walsh, BM (reprint author), Boston Univ, Dept Mech Engn & Ctr, Boston, MA 02215 USA.
EM bwalsh@bu.edu
RI Porter, Frederick/D-3501-2012; Collier, Michael/I-4864-2013
OI Porter, Frederick/0000-0002-6374-1119; Collier,
Michael/0000-0001-9658-6605
NR 60
TC 0
Z9 0
U1 6
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2016
VL 121
IS 4
BP 3353
EP 3361
DI 10.1002/2016JA022348
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DR5RO
UT WOS:000379960300037
ER
PT J
AU Liemohn, MW
Balikhin, M
Kepko, L
Rodger, A
Wang, YM
AF Liemohn, Michael W.
Balikhin, Michael
Kepko, Larry
Rodger, Alan
Wang, Yuming
TI Appreciation of the 2015 JGR Space Physics peer reviewers
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Editorial Material
AB The Editors of the Journal of Geophysical Research Space Physics extend their deepest gratitude to the 1506 scientists that have peer reviewed one or more manuscripts for the journal.
C1 [Liemohn, Michael W.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Balikhin, Michael] Univ Sheffield, Dept Automat Control & Syst Engn, Sheffield, S Yorkshire, England.
[Kepko, Larry] NASA, Goddard Space Flight Ctr, Space Weather Lab, Heliophys Sci Div, Greenbelt, MD USA.
[Rodger, Alan] Climate Change Risk & Resilience, Cambridge, England.
[Wang, Yuming] Univ Sci & Technol China, Sch Earth & Space Sci, Hefei, Peoples R China.
RP Liemohn, MW (reprint author), Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
EM liemohn@umich.edu
NR 0
TC 0
Z9 0
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2016
VL 121
IS 4
BP 3824
EP 3863
DI 10.1002/2016JA022705
PG 40
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DR5RO
UT WOS:000379960300069
ER
PT J
AU He, H
Vinnikov, KY
Li, C
Krotkov, NA
Jongeward, AR
Li, ZQ
Stehr, JW
Hains, JC
Dickerson, RR
AF He, Hao
Vinnikov, Konstantin Y.
Li, Can
Krotkov, Nickolay A.
Jongeward, Andrew R.
Li, Zhanqing
Stehr, Jeffrey W.
Hains, Jennifer C.
Dickerson, Russell R.
TI Response of SO2 and particulate air pollution to local and regional
emission controls: A case study in Maryland
SO EARTHS FUTURE
LA English
DT Article
ID OZONE MONITORING INSTRUMENT; UNITED-STATES; AEROSOL PRODUCTS; NOX
EMISSIONS; TRACE GAS; PROFILES; CAMPAIGN; SULFATE; TRENDS; MODIS
AB This paper addresses the questions of what effect local regulations can have on pollutants with different lifetimes and how surface observations and remotely sensed data can be used to determine the impacts. We investigated the decadal trends of tropospheric sulfur dioxide (SO2) and aerosol pollution over Maryland and its surrounding states, using surface, aircraft, and satellite measurements. Aircraft measurements indicated fewer isolated SO2 plumes observed in summers, a similar to 40% decrease of column SO2, and a similar to 20% decrease of atmospheric optical depth (AOD) over Maryland after the implementation of local regulations on sulfur emissions from power plants (similar to 90% reduction from 2010). Surface observations of SO2 and particulate matter ( PM) concentrations in Maryland show similar trends. OMI SO2 and MODIS AOD observations were used to investigate the column contents of air pollutants over the eastern U.S.; these indicate decreasing trends in column SO2 (similar to 60% decrease) and AOD (similar to 20% decrease). The decrease of upwind SO2 emissions also reduced aerosol loadings over the downwind Atlantic Ocean near the coast by similar to 20%, while indiscernible changes of the SO2 column were observed. A step change of SO2 emissions in Maryland starting in 2009-2010 had an immediate and profound benefit in terms of local surface SO2 concentrations but a modest impact on aerosol pollution, indicating that short-lived pollutants are effectively controlled locally, while long-lived pollutants require regional measures.
C1 [He, Hao; Vinnikov, Konstantin Y.; Jongeward, Andrew R.; Li, Zhanqing; Stehr, Jeffrey W.; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Li, Can; Li, Zhanqing; Dickerson, Russell R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Li, Can; Krotkov, Nickolay A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Hains, Jennifer C.] Maryland Dept Environm, Baltimore, MD 21224 USA.
RP He, H (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
EM haohe@umd.edu
RI Dickerson, Russell/F-2857-2010; Krotkov, Nickolay/E-1541-2012; Li,
Zhanqing/F-4424-2010
OI Dickerson, Russell/0000-0003-0206-3083; Krotkov,
Nickolay/0000-0001-6170-6750; Li, Zhanqing/0000-0001-6737-382X
FU Maryland Department of the Environment (MDE); NASA through a GEO-CAPE
grant [NNX12AD03A]; NASA AQAST; NASQ Aura Science Team [NNX11AK34G,
NNX12AI18G]
FX We thank the Maryland Department of the Environment (MDE) for support of
the RAMMPP project. We thank Dr. D. Goldberg for helpful comments. K.
Vinnikov acknowledges NASA support through a GEO-CAPE grant NNX12AD03A.
This research was also supported by NASA AQAST and NASQ Aura Science
Team grants NNX11AK34G and NNX12AI18G. We acknowledge the AERONET Team
for the production of the data used in this research. CEMS data of
SO2 and CO2 emissions from power plants are
available at the EPA Clean Air Markets Program database
(http://ampd.epa.gov/ampd). Observations of surface SO2 and
PM2.5 have been obtained freely from the EPA Air quality
System network website (https://ofmext.epa.gov/AQDMRS/aqdmrs.html).
Aircraft measurements are available at the UMD RAMMPP website
(http://www.atmos.umd.edu/-RAMMPP, per request). AERONET AOD
observations are available through the NASA AERONET website
(http://aeronet.gsfc.nasa.gov). Operation OMI SO2 products have been
obtained from the NASA Goddard Earth Sciences Data and Information
Service Center (http://daac.gsfc.nasa.gov/). The MODIS level 3 products
are available from the NASA Level 1 and Atmosphere Archive and
Distribution System (http://ladsweb.nascom.nasa.gov/).
NR 42
TC 2
Z9 2
U1 7
U2 14
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2328-4277
J9 EARTHS FUTURE
JI Earth Future
PD APR
PY 2016
VL 4
IS 4
BP 94
EP 109
DI 10.1002/2015EF000330
PG 16
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA DR1MD
UT WOS:000379668700001
ER
PT J
AU Lacelle, D
Lapalme, C
Davila, AF
Pollard, W
Marinova, M
Heldmann, J
McKay, CP
AF Lacelle, Denis
Lapalme, Caitlin
Davila, Alfonso F.
Pollard, Wayne
Marinova, Margarita
Heldmann, Jennifer
McKay, Christopher P.
TI Solar Radiation and Air and Ground Temperature Relations in the Cold and
Hyper-Arid Quartermain Mountains, McMurdo Dry Valleys of Antarctica
SO PERMAFROST AND PERIGLACIAL PROCESSES
LA English
DT Article
DE ground temperatures; surface offset; thermal offset; Quartermain
Mountains; McMurdo Dry Valleys; Antarctica
ID ACTIVE-LAYER; PERMAFROST DISTRIBUTION; SURFACE-TEMPERATURE; CLIMATE
HISTORY; YUKON-TERRITORY; MACKENZIE DELTA; THERMAL OFFSET; TAYLOR
VALLEY; TREE LINE; ICE
AB This study compares the relations between solar radiation and air and ground temperatures in the Quartermain Mountains of the McMurdo Dry Valleys of Antarctica with those in ice-free Victoria Land and Arctic Canada. The surface offset is near 0 degrees C at all sites in the Quartermain Mountains and other sites in coastal Victoria Land, whereas the thermal offset is near 0 degrees C at shallow ice table depths (<20 cm) and near 1 degrees C for ice tables deeper than the depth of diurnal temperature variation. The surface and thermal offsets in Victoria Land differ markedly from those in Arctic Canada, which are generally characterised by a positive surface offset and a negative thermal offset. These important differences highlight the effects of a lack of vegetation, surface organic layer, snow cover and moisture content in near-surface soils on the direction and magnitude of surface and thermal offsets. Summer ground surface temperatures in the Quartermain Mountains correlate strongly with incoming solar radiation. Based on measured ground surface temperatures and modelled potential incoming solar radiation, two zones with distinct ground surface temperatures are defined in the Quartermain Mountains: (i) perennially cryotic zones (PCZs) characterised by ground surface temperatures always below 0 degrees C; and (ii) seasonally non-cryotic zones (NCZs) characterised by ground surface temperatures > 0 degrees C for at least a few hours. Soils in the PCZs experience water exchange through vapour diffusion, whereas soils in the NCZs contain features associated with liquid water activity, such as increased soil moisture and frozen ponds recharged by snow/glacier meltwater. Copyright (c) 2015 John Wiley & Sons, Ltd.
C1 [Lacelle, Denis; Lapalme, Caitlin] Univ Ottawa, Dept Geog, 60 Univ St, Ottawa, ON K1S 6N5, Canada.
[Davila, Alfonso F.] SETI Inst, Carl Sagan Ctr, Mountain View, CA USA.
[Pollard, Wayne] McGill Univ, Dept Geog, Montreal, PQ, Canada.
[Marinova, Margarita; Heldmann, Jennifer; McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA USA.
RP Lacelle, D (reprint author), Univ Ottawa, Dept Geog, 60 Univ St, Ottawa, ON K1S 6N5, Canada.
EM dlacelle@uottawa.ca
OI Lacelle, Denis/0000-0002-6691-8717
FU NASA's Astrobiology Science and Technology for Exploring Planets (ASTEP)
program; Natural Sciences and Engineering Research Council of Canada
(NSERC) Discovery Grant
FX Fieldwork in the Quartermain Mountains was supported by NASA's
Astrobiology Science and Technology for Exploring Planets (ASTEP)
program and operated by the National Science Foundation (NSF) Office of
Polar Programs. An Natural Sciences and Engineering Research Council of
Canada (NSERC) Discovery Grant provided financial support for the data
analyses. We thank the Editor (J. Murton), Associate Editor (K. Hinkel)
and the two anonymous reviewers for their constructive comments.
NR 50
TC 3
Z9 3
U1 6
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1045-6740
EI 1099-1530
J9 PERMAFROST PERIGLAC
JI Permafrost Periglacial Process.
PD APR
PY 2016
VL 27
IS 2
BP 163
EP 176
DI 10.1002/ppp.1859
PG 14
WC Geography, Physical; Geology
SC Physical Geography; Geology
GA DP3XV
UT WOS:000378430300002
ER
PT J
AU Takacs, LL
Suarez, MJ
Todling, R
AF Takacs, Lawrence L.
Suarez, Max J.
Todling, Ricardo
TI Maintaining atmospheric mass and water balance in reanalyses
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE renalysis; incremental analysis update; data assimilation; mass
conservation
ID DATA ASSIMILATION SYSTEM; ERA-INTERIM; ENERGY; TRANSPORTS; OCEAN; LAND
AB This study describes the modifications made to the Goddard Earth Observing System (GEOS) Atmospheric Data Assimilation System (ADAS) to conserve atmospheric dry-air mass and to guarantee that the net source of water from precipitation and surface evaporation equals the change in total atmospheric water. The modifications involve changes to both the atmospheric model and the analysis procedure. In the model, sources and sinks of water are included in the continuity equation; in the analysis, constraints are imposed to penalize (and thus minimize) analysis increments of dry-air mass. Finally, changes are also required to the Incremental Analysis Update (IAU) procedure. The effects of these modifications are evaluated separately in free-running and assimilation experiments. Results are also presented from a multiyear reanalysis (Version 2 of the Modern Era Retrospective-Analysis for Research and Applications: MERRA-2) that uses the modified system.
C1 [Takacs, Lawrence L.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Takacs, Lawrence L.; Suarez, Max J.; Todling, Ricardo] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
[Suarez, Max J.] Univ Space Res Assoc, Columbia, MD USA.
RP Todling, R (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM Ricardo.Todling@nasa.gov
NR 19
TC 10
Z9 10
U1 0
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2016
VL 142
IS 697
BP 1565
EP 1573
DI 10.1002/qj.2763
PN B
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP3LR
UT WOS:000378395500001
ER
PT J
AU Souza, VM
Vieira, LEA
Medeiros, C
Da Silva, LA
Alves, LR
Koga, D
Sibeck, DG
Walsh, BM
Kanekal, SG
Jauer, PR
Rockenbach, M
Dal Lago, A
Silveira, MVD
Marchezi, JP
Mendes, O
Gonzalez, WD
Baker, DN
AF Souza, V. M.
Vieira, L. E. A.
Medeiros, C.
Da Silva, L. A.
Alves, L. R.
Koga, D.
Sibeck, D. G.
Walsh, B. M.
Kanekal, S. G.
Jauer, P. R.
Rockenbach, M.
Dal Lago, A.
Silveira, M. V. D.
Marchezi, J. P.
Mendes, O.
Gonzalez, W. D.
Baker, D. N.
TI A neural network approach for identifying particle pitch angle
distributions in Van Allen Probes data
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID OUTER RADIATION BELT; RELATIVISTIC ELECTRONS; ULTRARELATIVISTIC
ELECTRONS; MAGNETIC RECONNECTION; EARTHS MAGNETOPAUSE; GEOMAGNETIC
STORMS; ACCELERATION
AB Analysis of particle pitch angle distributions (PADs) has been used as a means to comprehend a multitude of different physical mechanisms that lead to flux variations in the Van Allen belts and also to particle precipitation into the upper atmosphere. In this work we developed a neural network-based data clustering methodology that automatically identifies distinct PAD types in an unsupervised way using particle flux data. One can promptly identify and locate three well-known PAD types in both time and radial distance, namely, 90 degrees peaked, butterfly, and flattop distributions. In order to illustrate the applicability of our methodology, we used relativistic electron flux data from the whole month of November 2014, acquired from the Relativistic Electron-Proton Telescope instrument on board the Van Allen Probes, but it is emphasized that our approach can also be used with multiplatform spacecraft data. Our PAD classification results are in reasonably good agreement with those obtained by standard statistical fitting algorithms. The proposed methodology has a potential use for Van Allen belt's monitoring.
C1 [Souza, V. M.; Vieira, L. E. A.; Medeiros, C.; Da Silva, L. A.; Alves, L. R.; Koga, D.; Jauer, P. R.; Rockenbach, M.; Dal Lago, A.; Marchezi, J. P.; Mendes, O.; Gonzalez, W. D.] Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, Brazil.
[Sibeck, D. G.; Kanekal, S. G.; Silveira, M. V. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Walsh, B. M.] Boston Univ, Dept Mech Engn, Boston, MA 02215 USA.
[Walsh, B. M.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Baker, D. N.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
RP Souza, VM (reprint author), Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, Brazil.
EM vitor.souza@inpe.br
OI Alves, Livia/0000-0002-5680-7271
FU Sao Paulo Research Foundation (FAPESP) [2014/21229-9]
FX This work was funded by Sao Paulo Research Foundation (FAPESP) grant
2014/21229-9. Van Allen Probes data from the REPT instrument can be
found at www.rbsp-ect.lanl.gov/. ACE magnetic field data are freely
available at http://www.srl.caltech.edu/ACE/ASC/level2/index.html.Dst
index data can be found at http://wdc.kugi.kyoto-u.ac.jp/dstdir/.
NR 29
TC 0
Z9 0
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD APR
PY 2016
VL 14
IS 4
BP 275
EP 284
DI 10.1002/2015SW001349
PG 10
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA DP0CI
UT WOS:000378154900002
ER
PT J
AU Elmendorf, SC
Jones, KD
Cook, BI
Diez, JM
Enquist, CAF
Hufft, RA
Jones, MO
Mazer, SJ
Miller-Rushing, AJ
Moore, DJP
Schwartz, MD
Weltzin, JF
AF Elmendorf, Sarah C.
Jones, Katherine D.
Cook, Benjamin I.
Diez, Jeffrey M.
Enquist, Carolyn A. F.
Hufft, Rebecca A.
Jones, Matthew O.
Mazer, Susan J.
Miller-Rushing, Abraham J.
Moore, David J. P.
Schwartz, Mark D.
Weltzin, Jake F.
TI The plant phenology monitoring design for The National Ecological
Observatory Network
SO ECOSPHERE
LA English
DT Article
DE long-term monitoring; NEON; open-source data; plant phenology; sample
design; Special Feature: NEON Design
ID CLIMATE-CHANGE; UNITED-STATES; FORECASTING PHENOLOGY;
RESOURCE-MANAGEMENT; SPECIES RESPONSES; SPRING PHENOLOGY; NORTH-AMERICA;
ONSET; TEMPERATURE; VARIABILITY
AB Phenology is an integrative science that comprises the study of recurring biological activities or events. In an era of rapidly changing climate, the relationship between the timing of those events and environmental cues such as temperature, snowmelt, water availability, or day length are of particular interest. This article provides an overview of the observer-based plant phenology sampling conducted by the U.S. National Ecological Observatory Network (NEON), the resulting data, and the rationale behind the design. Trained technicians will conduct regular in situ observations of plant phenology at all terrestrial NEON sites for the 30-yr life of the observatory. Standardized and coordinated data across the network of sites can be used to quantify the direction and magnitude of the relationships between phenology and environmental forcings, as well as the degree to which these relationships vary among sites, among species, among phenophases, and through time. Vegetation at NEON sites will also be monitored with tower-based cameras, satellite remote sensing, and annual high-resolution airborne remote sensing. Ground-based measurements can be used to calibrate and improve satellite-derived phenometrics. NEON's phenology monitoring design is complementary to existing phenology research efforts and citizen science initiatives throughout the world and will produce interoperable data. By collocating plant phenology observations with a suite of additional meteorological, biophysical, and ecological measurements (e.g., climate, carbon flux, plant productivity, population dynamics of consumers) at 47 terrestrial sites, the NEON design will enable continental-scale inference about the status, trends, causes, and ecological consequences of phenological change.
C1 [Elmendorf, Sarah C.; Jones, Katherine D.] Natl Ecol Observ Network, 1685 38th St, Boulder, CO 80301 USA.
[Elmendorf, Sarah C.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA.
[Cook, Benjamin I.] NASA Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Diez, Jeffrey M.] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA.
[Enquist, Carolyn A. F.] USA Natl Phenol Network, Natl Coordinating Off, 1955 E 6th St, Tucson, AZ 85719 USA.
[Enquist, Carolyn A. F.] US Geol Survey, DOI Southwest Climate Sci Ctr, 1064 E Lowell St, Tucson, AZ 85721 USA.
[Hufft, Rebecca A.] Denver Bot Gardens, 909 York St, Denver, CO 80206 USA.
[Jones, Matthew O.] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA.
[Mazer, Susan J.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA.
[Miller-Rushing, Abraham J.] Natl Pk Serv, Acad Natl Pk & Schood Educ & Res Ctr, Bar Harbor, ME 04660 USA.
[Moore, David J. P.] Univ Arizona, Sch Nat Resources & Environm, 1064 East Lowell St, Tucson, AZ 85721 USA.
[Schwartz, Mark D.] Univ Wisconsin, Dept Geog, POB 413, Milwaukee, WI 53201 USA.
[Weltzin, Jake F.] US Geol Survey, 1955 East 6th St, Tucson, AZ 85721 USA.
RP Elmendorf, SC (reprint author), Natl Ecol Observ Network, 1685 38th St, Boulder, CO 80301 USA.; Elmendorf, SC (reprint author), Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA.
EM selmendorf@neoninc.org
RI Cook, Benjamin/H-2265-2012
FU National Science Foundation [EF-1029808]
FX We thank Shirley Papuga, Yuri Springer, and Lee Stanish for helpful
comments on the manuscript. Any use of trade, product, or firm names is
for descriptive purposes only and does not imply endorsement by the U.S.
Government. This material is based upon work supported by the National
Science Foundation under Cooperative Service Agreement EF-1029808.
NR 70
TC 1
Z9 1
U1 8
U2 18
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2150-8925
J9 ECOSPHERE
JI Ecosphere
PD APR
PY 2016
VL 7
IS 4
AR e01303
DI 10.1002/ecs2.1303
PG 16
WC Ecology
SC Environmental Sciences & Ecology
GA DN6VA
UT WOS:000377213400010
ER
PT J
AU Clem, MM
Zaman, KBMQ
Fagan, AF
AF Clem, Michelle M.
Zaman, K. B. M. Q.
Fagan, Amy F.
TI Variation of shock-spacing during screech stage-jumps
SO INTERNATIONAL JOURNAL OF AEROACOUSTICS
LA English
DT Article
DE screech; stage-jump; hysteresis; supersonic jets; shadowgraphy; flow
visualization
ID SUPERSONIC JET SCREECH; NUMERICAL-SIMULATION; CIRCULAR JETS; NOISE;
MODE; OSCILLATION; GENERATION
AB Flow visualization is used to investigate shock-spacings in a supersonic jet during stage-jumps associated with the screech phenomenon. Conventional schlieren and shadowgraphy techniques as well as a new projection focusing schlieren technique are employed. Both time-averaged and instantaneous snapshots of the flow field are analyzed for a 37.6mm round convergent nozzle over the jet Mach number range of 1.0= 1 keV, and for whistler mode chorus waves, structures appear for energies >2 keV at L = 4.6 and above 200 eV for L = 6.8. The results obtained in the present work will be helpful in the study of diffusion curves and will have important consequences for diffuse aurora and pancake distributions. (C) 2016 AIP Publishing LLC.
C1 [Tripathi, A. K.; Singhal, R. P.] Banaras Hindu Univ, Indian Inst Technol, Dept Phys, Varanasi 221005, Uttar Pradesh, India.
[Khazanov, G. V.; Avanov, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Avanov, L. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Khazanov, GV (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM aktrip2001@yahoo.co.in; rpsiitbhu@yahoo.com; George.V.Khazanov@nasa.gov;
levon.a.avanov@nasa.gov
FU Planetary Sciences and Exploration Programme, Indian Space Research
Organization (ISRO), PRL, Ahmedabad; NASA Van Allen Probes; NASA LWS
Program; Indian Institute of Technology (Banaras Hindu University),
India
FX This work was supported with financial assistance provided by the
Planetary Sciences and Exploration Programme, Indian Space Research
Organization (ISRO), PRL, Ahmedabad, under the sanctioned PLANEX project
scheme. Funding support for this study was also provided by NASA Van
Allen Probes (formerly known as the Radiation Belt Storm Probes (RBSP))
Project, the NASA LWS Program, and by the Indian Institute of Technology
(Banaras Hindu University), India. The data for this paper are available
from George V. Khazanov at george.v.khazanov@nasa.gov. Calculations
reported in the present work were carried out at the Computer Centre,
Banaras Hindu University.
NR 33
TC 1
Z9 1
U1 1
U2 2
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD APR
PY 2016
VL 23
IS 4
AR 042101
DI 10.1063/1.4944920
PG 9
WC Physics, Fluids & Plasmas
SC Physics
GA DL7YE
UT WOS:000375855500005
ER
PT J
AU Shiri, R
Stein, R
Murphy, K
Hagopian, K
Salari, S
Sankar, S
Hagopian, J
Showalter, M
Stevenson, T
Quijada, M
Threat, F
Friedlander, J
Dillon, T
Livas, J
AF Shiri, Ron
Stein, Ryan
Murphy, Kaitlin
Hagopian, Kimberly
Salari, Shirin
Sankar, Shannon
Hagopian, John
Showalter, Matthew
Stevenson, Thomas
Quijada, Manuel
Threat, Felix
Friedlander, Jay
Dillon, Thomas
Livas, Jeffrey
TI Fabrication of petal-shaped masks for suppression of the on-axis Poisson
spot in telescope systems
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID OCCULTER
AB The presence of a bright (Poisson) spot in the geometrical shadow of circular/spherical shapes has been known for the past two centuries. A broad class of telescopes that involve simultaneous transmit and receive require suppression of the reflected light from the secondary mirror on the detector. For instance, the on-axis design of optical telescope for the evolved Laser Interferometric Space Antenna (eLISA), a re-scoped version of the baseline LISA mission concept, requires suppression of reflected laser light from the secondary mirror on the detector. In the past few years, the hypergaussian functions with petal-shaped realization have been shown to significantly suppress intensity along the optical axis. This work reports on fabrication of a series of petal-shaped masks using a variety of techniques such as 3D printing, photolithography, and wire Electro Discharge Machining. These masks are designed and fabricated to operate in the range of Fresnel numbers between 4 and 120. This paper discusses the challenges, successes, and failures of each fabrication technique and the optical performance of typical masks with suggestions for potential follow up work.
C1 [Shiri, Ron; Murphy, Kaitlin; Hagopian, Kimberly; Salari, Shirin; Hagopian, John; Quijada, Manuel; Threat, Felix] NASA, Goddard Space Flight Ctr, Opt Branch, Greenbelt, MD 20771 USA.
[Stein, Ryan; Sankar, Shannon; Livas, Jeffrey] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
[Sankar, Shannon] Univ Space Res Assoc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Showalter, Matthew] NASA, Goddard Space Flight Ctr, Adv Mfg Branch, Greenbelt, MD 20771 USA.
[Stevenson, Thomas] NASA, Goddard Space Flight Ctr, Detector Syst Branch, Greenbelt, MD 20771 USA.
[Friedlander, Jay] NASA, Goddard Space Flight Ctr, Astrophys Sci Lab, Greenbelt, MD 20771 USA.
[Dillon, Thomas] Univ Delaware, Dept Elect & Comp Engn, Newark, DC 19716 USA.
RP Shiri, R (reprint author), NASA, Goddard Space Flight Ctr, Opt Branch, Greenbelt, MD 20771 USA.
FU NASA [11-SAT11-0027 NNH11ZDA001N]
FX This work is supported in part through NASA Grant 11-SAT11-0027
NNH11ZDA001N "Research Opportunities in Space and Earth Sciences"
(ROSES-2011) for Strategic Astrophysics Technology (SAT).
NR 7
TC 0
Z9 0
U1 2
U2 2
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0034-6748
EI 1089-7623
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD APR
PY 2016
VL 87
IS 4
AR 043112
DI 10.1063/1.4945793
PG 6
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA DL7TH
UT WOS:000375842500015
PM 27131659
ER
PT J
AU Wedemeyer, S
Bastian, T
Brajsa, R
Hudson, H
Fleishman, G
Loukitcheva, M
Fleck, B
Kontar, EP
De Pontieu, B
Yagoubov, P
Tiwari, SK
Soler, R
Black, JH
Antolin, P
Scullion, E
Gunar, S
Labrosse, N
Ludwig, HG
Benz, AO
White, SM
Hauschildt, P
Doyle, JG
Nakariakov, VM
Ayres, T
Heinzel, P
Karlicky, M
Van Doorsselaere, T
Gary, D
Alissandrakis, CE
Nindos, A
Solanki, SK
van der Voort, LR
Shimojo, M
Kato, Y
Zaqarashvili, T
Perez, E
Selhorst, CL
Barta, M
AF Wedemeyer, S.
Bastian, T.
Brajsa, R.
Hudson, H.
Fleishman, G.
Loukitcheva, M.
Fleck, B.
Kontar, E. P.
De Pontieu, B.
Yagoubov, P.
Tiwari, S. K.
Soler, R.
Black, J. H.
Antolin, P.
Scullion, E.
Gunar, S.
Labrosse, N.
Ludwig, H. -G.
Benz, A. O.
White, S. M.
Hauschildt, P.
Doyle, J. G.
Nakariakov, V. M.
Ayres, T.
Heinzel, P.
Karlicky, M.
Van Doorsselaere, T.
Gary, D.
Alissandrakis, C. E.
Nindos, A.
Solanki, S. K.
van der Voort, L. Rouppe
Shimojo, M.
Kato, Y.
Zaqarashvili, T.
Perez, E.
Selhorst, C. L.
Barta, M.
TI Solar Science with the Atacama Large Millimeter/Submillimeter Array-A
New View of Our Sun
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun; Photosphere; Chromosphere; Corona; Magnetohydrodynamics; Radiative
transfer; Flares; Prominences
ID HARD X-RAY; REGION-IMAGING-SPECTROGRAPH; QUASI-PERIODIC PULSATIONS;
MILLIMETER-INTERFEROMETER OBSERVATIONS; SLOW MAGNETOACOUSTIC
OSCILLATIONS; CORONAL DIAGNOSTIC SPECTROMETER; HIGH-RESOLUTION
OBSERVATIONS; DYNAMIC HYDROGEN IONIZATION; NEAR-INFRARED OBSERVATIONS;
PROMINENCE FINE-STRUCTURES
AB The Atacama Large Millimeter/submillimeter Array (ALMA) is a new powerful tool for observing the Sun at high spatial, temporal, and spectral resolution. These capabilities can address a broad range of fundamental scientific questions in solar physics. The radiation observed by ALMA originates mostly from the chromosphere-a complex and dynamic region between the photosphere and corona, which plays a crucial role in the transport of energy and matter and, ultimately, the heating of the outer layers of the solar atmosphere. Based on first solar test observations, strategies for regular solar campaigns are currently being developed. State-of-the-art numerical simulations of the solar atmosphere and modeling of instrumental effects can help constrain and optimize future observing modes for ALMA. Here we present a short technical description of ALMA and an overview of past efforts and future possibilities for solar observations at submillimeter and millimeter wavelengths. In addition, selected numerical simulations and observations at other wavelengths demonstrate ALMA's scientific potential for studying the Sun for a large range of science cases.
C1 [Wedemeyer, S.; De Pontieu, B.; van der Voort, L. Rouppe; Kato, Y.] Univ Oslo, Inst Theoret Astrophys, Postboks 1029, N-0315 Oslo, Norway.
[Wedemeyer, S.; Brajsa, R.; Barta, M.] ASCR, Astron Inst, Czech Node, European ARC, Ondrejov, Czech Republic.
[Bastian, T.] NRAO, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
[Brajsa, R.] Univ Zagreb, Fac Geodesy, Hvar Observ, Zagreb 41000, Croatia.
[Hudson, H.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
[Hudson, H.; Kontar, E. P.; Labrosse, N.; Perez, E.] Univ Glasgow, Sch Phys & Astron, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Fleishman, G.; Gary, D.] New Jersey Inst Technol, Dept Phys, Ctr Solar Terr Res, 323 MLK Blvd, Newark, NJ 07102 USA.
[Loukitcheva, M.] St Petersburg Univ, Astron Inst, Univ Skii Pr 28, St Petersburg 198504, Russia.
[Loukitcheva, M.; Solanki, S. K.] Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[Fleck, B.] NASA, ESA Sci Operat Dept, Goddard Space Flight Ctr, Greenbelt, MD USA.
[De Pontieu, B.] Lockheed Martin Solar & Astrophys Lab, 3251 Hanover St,Org A021S,B-252, Palo Alto, CA 94304 USA.
[Yagoubov, P.] European Org Astron Res Southern Hemisphere ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Tiwari, S. K.] NASA, Marshall Space Flight Ctr, ZP 13, Huntsville, AL 35805 USA.
[Soler, R.] Univ Illes Balears, Dept Fis, Palma De Mallorca 07122, Spain.
[Black, J. H.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden.
[Antolin, P.; Shimojo, M.] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Scullion, E.] Univ Dublin Trinity Coll, Coll Green, Dublin 2, Ireland.
[Gunar, S.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
[Gunar, S.; Heinzel, P.; Karlicky, M.; Barta, M.] Acad Sci Czech Republic, Astron Inst, Fricova 298, Ondrejov 25165, Czech Republic.
[Ludwig, H. -G.] ZAH, Landessternwarte Konigstuhl 12, D-69117 Heidelberg, Germany.
[Benz, A. O.] FHNW, Inst Technol 4D, Windisch, Switzerland.
[White, S. M.] AFRL, Space Vehicles Directorate, 3550 Aberdeen Ave SE,Bldg 427, Kirtland AFB, NM 87117 USA.
[Hauschildt, P.] Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Doyle, J. G.] Coll Hill, Armagh Observ, Armagh BT61 9DG, North Ireland.
[Nakariakov, V. M.] Univ Warwick, Dept Phys, Ctr Fus Space & Astrophys, Coventry CV4 7AL, W Midlands, England.
[Ayres, T.] Univ Colorado, Ctr Astrophys & Space Astron, Campus Box 391, Boulder, CO 80309 USA.
[Van Doorsselaere, T.] Katholieke Univ Leuven, Dept Math, Ctr Math Plasma Astrophys, Celestijnenlaan 200B Bus 2400, B-3000 Leuven, Belgium.
[Alissandrakis, C. E.; Nindos, A.] Univ Ioannina, Dept Phys, POB 1186, GR-45110 Ioannina, Greece.
[Solanki, S. K.] Kyung Hee Univ, Sch Space Res, Yongin, Gyeonggi, South Korea.
[Zaqarashvili, T.] Graz Univ, Inst Phys, Univ Pl 5, A-8010 Graz, Austria.
[Zaqarashvili, T.] Ilia State Univ, Abastumani Astrophys Observ, Univ St 2, Tbilisi, Rep of Georgia.
[Selhorst, C. L.] Univ Vale Paraiba UNIVAP, Av Shishima Hifumi 2911, BR-12244000 Sao Jose Dos Campos, SP, Brazil.
RP Wedemeyer, S (reprint author), Univ Oslo, Inst Theoret Astrophys, Postboks 1029, N-0315 Oslo, Norway.; Wedemeyer, S (reprint author), ASCR, Astron Inst, Czech Node, European ARC, Ondrejov, Czech Republic.
EM svenwe@astro.uio.no
RI Shimojo, Masumi/J-2605-2016; Nakariakov, Valery/E-2375-2013; Selhorst,
Caius/E-9619-2010; Kontar, Eduard/B-7897-2008; Barta,
Miroslav/C-7069-2012; Karlicky, Marian/G-9023-2014; Gunar,
Stanislav/G-9012-2014; Heinzel, Petr/G-9014-2014; Labrosse,
Nicolas/B-2670-2010; Loukitcheva, Maria/I-6110-2013; Wedemeyer,
Sven/F-3957-2010
OI Shimojo, Masumi/0000-0002-2350-3749; Nakariakov,
Valery/0000-0001-6423-8286; Selhorst, Caius/0000-0002-5897-5236; Kontar,
Eduard/0000-0002-8078-0902; Labrosse, Nicolas/0000-0002-4638-157X;
Loukitcheva, Maria/0000-0001-5246-9044; Wedemeyer,
Sven/0000-0002-5006-7540
FU Faculty of Mathematics and Natural Sciences of the University of Oslo,
Norway [UiO-PES2020]; Research Council of Norway [221767/F20]; European
Commission [284461, 312495]; Croatian Science Foundation [6212]; NSF
[AGS-1250374, AGS-1262772]; NASA [NNX14AC87G]; Saint-Petersburg State
University [6.0.26.2010, 6.37.343.2015, 6.42.1428.2015]; European
Commission through the CIG [PCIG-GA-2011-304265]; GACR [13-24782S];
Marie Curie RadioSun project [PIRSES-GA-2011-295272]; MINECO; FEDER
funds [AYA2011-22846]; "Juan de la Cierva" grant [JCI-2012-13594]; MECD
[CEF11-0012]; CAIB ("Grups Competitius" program); UIB ("Vicerectorat
d'Investigacio i Postgrau"); NASA; Irish Research Council; STFC
[ST/L000741/1, ST/L000733/1]; European Community [606862]; N. Ireland
Dept. of Culture, Arts and Leisure; FWO Vlaanderen; CHARM (Belspo) [IAP
P7/08]; KU Leuven [GOA-2015-014]; European Union (European Social
Fund-ESF); Greek national funds through the Operational Program
"Education and Lifelong Learning" of the National Strategic Reference
Framework (NSRF)-Research Funding Program: "Thales. Investing in
knowledge society through the European Social Fund"; FWF (the Austrian
Fonds zur Forderung der Wissenschaftlichen Forschung) [P26181-N27]; Sao
Paulo Research Foundation (FAPESP) [2014/10489-0]
FX This review was written in connection with the Solar Simulations for the
Atacama Large Millimeter Observatory Network (SSALMON,
http://www.ssalmon.uio.no). We are grateful to the many colleagues who
are working actively on realising the solar observing modes for ALMA as
part of CSV/EOC activities carried out by the solar development teams of
the NA/EU/EA-ARCs and JAO. In particular, we would like to thank A.
Remijan and R. Hills for helpful comments. S. Wedemeyer acknowledges
support (UiO-PES2020) by the Faculty of Mathematics and Natural Sciences
of the University of Oslo, Norway, and the Research Council of Norway
(grant 221767/F20). R. Brajsa was supported by the European Commission
FP7 with the projects eHEROES (284461, 2012-2015) and SOLARNET (312495,
2013-2017), as well as by the Croatian Science Foundation (project 6212
"Solar and Stellar Variability"). G. Fleishman is supported by NSF
grants AGS-1250374 and AGS-1262772 and NASA grant NNX14AC87G to the New
Jersey Institute of Technology. M. Loukitcheva acknowledges
Saint-Petersburg State University for research grants 6.0.26.2010,
6.37.343.2015 and 6.42.1428.2015, and grant RFBR 15-02-03835. M. Barta
thanks for the support of the European Commission through the CIG grant
PCIG-GA-2011-304265 (SERAF) and GACR grant 13-24782S. M. Barta, M.
Karlicky, E. Kontar and V. M. Nakariakov acknowledge the Marie Curie
PIRSES-GA-2011-295272 RadioSun project. R. Soler acknowledges support
from MINECO and FEDER funds (AYA2011-22846), from a "Juan de la Cierva"
grant (JCI-2012-13594), from MECD (CEF11-0012), from CAIB ("Grups
Competitius" program), and UIB ("Vicerectorat d'Investigacio i
Postgrau"). S. K. Tiwari is supported by appointment to the NASA
Postdoctoral Program at the NASA/MSFC, administered by ORAU through a
contract with NASA. E. Scullion is a Government of Ireland Post-doctoral
Research Fellow supported by the Irish Research Council. N. Labrosse
acknowledges support from STFC grant ST/L000741/1, and, together with H.
Hudson, funding from the European Community's Seventh Framework
Programme (FP7/2007-2013) under grant agreement no. 606862 (F-CHROMA).
Research at the Armagh Observatory is grant-aided by the N. Ireland
Dept. of Culture, Arts and Leisure. V. M. Nakariakov acknowledges the
STFC consolidated grant ST/L000733/1. T. Van Doorsselaere was supported
by an Odysseus grant of the FWO Vlaanderen, the IAP P7/08 CHARM (Belspo)
and the GOA-2015-014 (KU Leuven). A Nindos' work has been partly
co-financed by the European Union (European Social Fund-ESF) and Greek
national funds through the Operational Program "Education and Lifelong
Learning" of the National Strategic Reference Framework (NSRF)-Research
Funding Program: "Thales. Investing in knowledge society through the
European Social Fund". T. V. Zaqarashvili acknowledges FWF (the Austrian
Fonds zur Forderung der Wissenschaftlichen Forschung) project
P26181-N27. C. L. Selhorst acknowledges financial support from the Sao
Paulo Research Foundation (FAPESP), grant number 2014/10489-0. We
acknowledge usage of the SAO/NASA Astrophysics Data System (ADS).
NR 481
TC 6
Z9 6
U1 1
U2 9
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD APR
PY 2016
VL 200
IS 1-4
BP 1
EP 73
DI 10.1007/s11214-015-0229-9
PG 73
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DM1AP
UT WOS:000376077700001
ER
PT J
AU Kalina, EA
Friedrich, K
Motta, BC
Deierling, W
Stano, GT
Rydell, NN
AF Kalina, Evan A.
Friedrich, Katja
Motta, Brian C.
Deierling, Wiebke
Stano, Geoffrey T.
Rydell, Nezette N.
TI Colorado Plowable Hailstorms: Synoptic Weather, Radar, and Lightning
Characteristics
SO WEATHER AND FORECASTING
LA English
DT Article
ID LINEAR-POLARIZATION RADAR; 24 JUNE 2006; POLARIMETRIC RADAR; CONVECTIVE
STORMS; HAIL GROWTH; PART II; HYDROMETEOR CLASSIFICATION; SOUTHWESTERN
FRANCE; 3-BODY SCATTERING; MAPPING ARRAY
AB Synoptic weather, S-band dual-polarization radar, and total lightning observations are analyzed from four thunderstorms that produced "plowable" hail accumulations of 15-60 cm in localized areas of the Colorado Front Range. Results indicate that moist, relatively slow (5-15 m s(-1)) southwesterly-to-westerly flow at 500 hPa and postfrontal low-level upslope flow, with 2-m dewpoint temperatures of 11 degrees-19 degrees C at 1200 LST, were present on each plowable hail day. This pattern resulted in column-integrated precipitable water values that were 132 %-184% of the monthly means and freezing-level heights that were 100-700 m higher than average. Radar data indicate that between one and three maxima in reflectivity Z (68-75 dBZ) and 50-dBZ echo-top height (11-15 km MSL) occurred over the lifetime of each hailstorm. These maxima, which imply an enhancement in updraft strength, resulted in increased graupel and hail production and accumulating hail at the surface within 30 min of the highest echo tops. The hail core had Z similar to 70 dBZ, differential reflectivity ZDR from 0 to -4 dB, and correlation coefficient rho(HV) of 0.80-0.95. Time-height plots reveal that these minima in ZDR and rho(HV) gradually descended to the surface after originating at heights of 6-10 km MSL similar to 15-60 min prior to accumulating hailfall. Hail accumulations estimated from the radar data pinpoint the times and locations of plowable hail, with depths greater than 5 cm collocated with the plowable hail reports. Three of the four hail events were accompanied by lightning flash rates near the maximum observed thus far within the thunderstorm.
C1 [Kalina, Evan A.] NOAA, Earth Syst Res Lab, Div Phys Sci, 325 Broadway St, Boulder, CO 80305 USA.
[Kalina, Evan A.] NOAA, Atlantic Oceanog & Meteorol Lab, Hurricane Res Div, Miami, FL 33149 USA.
[Friedrich, Katja] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Motta, Brian C.] NOAA, NWS, Off Chief Learning Officer Boulder, Boulder, CO USA.
[Deierling, Wiebke] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Stano, Geoffrey T.] NASA, Shortterm Predict Res & Transit Ctr SPoRT ENSCO I, Huntsville, AL USA.
[Rydell, Nezette N.] NOAA, NWS, Boulder, CO USA.
RP Kalina, EA (reprint author), NOAA, Earth Syst Res Lab, Div Phys Sci, 325 Broadway St, Boulder, CO 80305 USA.
EM evan.kalina@noaa.gov
FU National Science Foundation [DGE-1144083]
FX We thank the employees of the National Weather Service Forecast Office
in Boulder for providing valuable feedback on this study. We also thank
Mike Dixon (NCAR) for his assistance in using the Radx C++ software
package for radar data processing, and Scott Ellis (NCAR) for his help
in using Solo II to view and edit the radar data. Feedback from three
anonymous reviewers greatly improved an earlier version of this
manuscript. This material is based upon work supported by the National
Science Foundation Graduate Research Fellowship program under
DGE-1144083. A portion of this research was performed while EAK held a
National Research Council Research Associateship Award at the Earth
System Research Laboratory and the Atlantic Oceanographic and
Meteorological Laboratory.
NR 87
TC 0
Z9 0
U1 10
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0882-8156
EI 1520-0434
J9 WEATHER FORECAST
JI Weather Forecast.
PD APR
PY 2016
VL 31
IS 2
BP 663
EP 693
DI 10.1175/WAF-D-15-0037.1
PG 31
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DM2ZJ
UT WOS:000376216300019
ER
PT J
AU Coffel, ED
Horton, RM
AF Coffel, Ethan D.
Horton, Radley M.
TI Reply to "Comment on 'Climate Change and the Impact of Extreme
Temperatures on Aviation'"
SO WEATHER CLIMATE AND SOCIETY
LA English
DT Letter
C1 [Coffel, Ethan D.] Columbia Univ, Dept Earth & Environm Sci, New York, NY USA.
[Coffel, Ethan D.; Horton, Radley M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Horton, Radley M.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
RP Coffel, ED (reprint author), 2880 Broadway, New York, NY 10025 USA.
EM ec2959@columbia.edu
NR 2
TC 0
Z9 0
U1 2
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1948-8327
EI 1948-8335
J9 WEATHER CLIM SOC
JI Weather Clim. Soc.
PD APR
PY 2016
VL 8
IS 2
BP 207
EP 208
DI 10.1175/WCAS-D-15-0063.1
PG 2
WC Environmental Studies; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DM1WV
UT WOS:000376138500002
ER
PT J
AU Abdul-Masih, M
Prsa, A
Conroy, K
Bloemen, S
Boyajian, T
Doyle, LR
Johnston, C
Kostov, V
Latham, DW
Matijevic, G
Shporer, A
Southworth, J
AF Abdul-Masih, Michael
Prsa, Andrej
Conroy, Kyle
Bloemen, Steven
Boyajian, Tabetha
Doyle, Laurance R.
Johnston, Cole
Kostov, Veselin
Latham, David W.
Matijevic, Gal
Shporer, Avi
Southworth, John
TI KEPLER ECLIPSING BINARY STARS. VIII. IDENTIFICATION OF FALSE POSITIVE
ECLIPSING BINARIES AND RE-EXTRACTION OF NEW LIGHT CURVES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; catalogs; methods: analytical; methods: data
analysis; methods: statistical; techniques: photometric
ID DATA RELEASE; CATALOG; I.
AB The Kepler mission has provided unprecedented, nearly continuous photometric data of similar to 200,000 objects in the similar to 105 deg(2) field of view (FOV) from the beginning of science operations in May of 2009 until the loss of the second reaction wheel in May of 2013. The Kepler Eclipsing Binary Catalog contains information including but not limited to ephemerides, stellar parameters, and analytical approximation fits for every known eclipsing binary system in the Kepler FOV. Using target pixel level data collected from Kepler in conjunction with the Kepler Eclipsing Binary Catalog, we identify false positives among eclipsing binaries, i.e., targets that are not eclipsing binaries themselves, but are instead contaminated by eclipsing binary sources nearby on the sky and show eclipsing binary signatures in their light curves. We present methods for identifying these false positives and for extracting new light curves for the true source of the observed binary signal. For each source, we extract three separate light curves for each quarter of available data by optimizing the signal-to-noise ratio, the relative percent eclipse depth, and the flux eclipse depth. We present 289 new eclipsing binaries in the Kepler FOV that were not targets for observation, and these have been added to the catalog. An online version of this catalog with downloadable content and visualization tools is maintained at http://keplerEBs.villanova.edu.
C1 [Abdul-Masih, Michael; Prsa, Andrej; Johnston, Cole; Matijevic, Gal] Villanova Univ, Dept Astrophys & Planetary Sci, 800 E Lancaster, Villanova, PA 19085 USA.
[Abdul-Masih, Michael] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA.
[Conroy, Kyle] Vanderbilt Univ, Dept Phys & Astron, VU Stn B 1807, Nashville, TN 37235 USA.
[Bloemen, Steven] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Boyajian, Tabetha] Yale Univ, JW Gibbs Lab, 260 Whitney Ave, New Haven, CT 06511 USA.
[Doyle, Laurance R.] Principia Coll, IMoP, Elsah, IL 62028 USA.
[Doyle, Laurance R.] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
[Kostov, Veselin] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Latham, David W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Shporer, Avi] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Southworth, John] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
RP Abdul-Masih, M (reprint author), Villanova Univ, Dept Astrophys & Planetary Sci, 800 E Lancaster, Villanova, PA 19085 USA.
OI Boyajian, Tabetha/0000-0001-9879-9313; Latham, David/0000-0001-9911-7388
FU NASA GO grant [14-K2GO1_2-0057]; Kepler mission via NASA [NNX13AB58A,
NNX11AB99A]; Smithsonian Astrophysical Observatory; Theodore Dunham, Jr.
Grant of the Fund for Astrophysical Research; NASA [NAS5-26555]; NASA
Office of Space Science [NNX09AF08G]; NASAs Science Mission Directorate
FX We gratefully acknowledge support from NASA GO grant 14-K2GO1_2-0057.
D.W.L. gratefully acknowledges support from the Kepler mission via NASA
Cooperative Agreements NNX13AB58A and NNX11AB99A with the Smithsonian
Astrophysical Observatory. The high-performance computational facility
used for this work was sponsored in part by the Theodore Dunham, Jr.
Grant of the Fund for Astrophysical Research. All of the data presented
in this paper were obtained from the Multimission Archive at the Space
Telescope Science Institute (MAST). STScI is operated by the Association
of Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555. Support for MAST for non-Hubble Space Telescope data is
provided by the NASA Office of Space Science via grant NNX09AF08G and by
other grants and contracts. Funding for this Discovery Mission is
provided by NASAs Science Mission Directorate.
NR 17
TC 1
Z9 1
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD APR
PY 2016
VL 151
IS 4
AR 101
DI 10.3847/0004-6256/151/4/101
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DL4LV
UT WOS:000375609100014
ER
PT J
AU Arulanantham, NA
Herbst, W
Cody, AM
Stauffer, JR
Rebull, LM
Agol, E
Windemuth, D
Marengo, M
Winn, JN
Hamilton, CM
Mundt, R
Johns-Krull, CM
Gutermuth, RA
AF Arulanantham, Nicole A.
Herbst, William
Cody, Ann Marie
Stauffer, John R.
Rebull, Luisa M.
Agol, Eric
Windemuth, Diana
Marengo, Massimo
Winn, Joshua N.
Hamilton, Catrina M.
Mundt, Reinhard
Johns-Krull, Christopher M.
Gutermuth, Robert A.
TI SEEING THROUGH THE RING: NEAR-INFRARED PHOTOMETRY OF V582 MON (KH 15D)
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE open clusters and associations: individual (NGC 2264); protoplanetary
disks; stars: individual (KH15D); stars: pre-main sequence
ID SPITZER-SPACE-TELESCOPE; NGC 2264; SPECTROSCOPIC BINARY; MYSTERIOUS
ECLIPSES; CLUSTER; DISK; VARIABILITY; EMISSION; STARS; OCCULTATIONS
AB We examine the light and color evolution of the T Tauri binary KH 15D through photometry obtained at wavelengths between 0.55 and 8.0 mu m. The data were collected with A Novel Dual Imaging CAMera (ANDICAM) on the 1.3 m SMARTS telescope at Cerro-Tololo Inter-American Observatory and with InfraRed Array Camera on the Spitzer Space Telescope. We show that the system's circumbinary ring, which acts as a screen that covers and uncovers different portions of the binary orbit as the ring precesses, has reached an orientation where the brighter component (star B) fully or nearly fully emerges during each orbital cycle. The fainter component (star A) remains fully occulted by the screen at all phases. The leading and trailing edges of the screen move across the sky at the same rate of similar to 15 m s(-1), consistent with expectation for a ring with a radius and width of similar to 4 au and a precession period of similar to 6500 years. Light and color variations continue to indicate that the screen is sharp edged and opaque at VRIJH wavelengths. However, we find an increasing transparency of the ring edge at 2.2, 3.6, and 4.5 mu m. Reddening seen at the beginning of the eclipse that occurred during the CSI 2264 campaign particularly suggests selective extinction by a population of large dust grains. Meanwhile, the gradual bluing observed while star B is setting is indicative of forward scattering effects at the edge of the ring. The spectral energy distribution of the system at its bright phase shows no evidence of infrared excess emission that can be attributed to radiation from the ring or other dust component out to 8 mu m.
C1 [Arulanantham, Nicole A.; Herbst, William] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA.
[Cody, Ann Marie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Stauffer, John R.; Rebull, Luisa M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Agol, Eric; Windemuth, Diana] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Marengo, Massimo] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Hamilton, Catrina M.] Dickinson Coll, Dept Phys & Astron, Carlisle, PA 17013 USA.
[Mundt, Reinhard] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Johns-Krull, Christopher M.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
[Gutermuth, Robert A.] Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA.
RP Arulanantham, NA (reprint author), Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA.
OI /0000-0002-0802-9145
FU NASA; CT Space Grant Consortium
FX This work is based in part on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. It has
also made use of the 1.3 m telescope operated by the SMARTS consortium
at Cerro Toloto Interamerican Observatory in Chile. We are grateful for
funding from the CT Space Grant Consortium that partially supported this
research. We are grateful to Wesleyan undergraduate student Rachel
Aronow for her help with this project.
NR 35
TC 1
Z9 1
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD APR
PY 2016
VL 151
IS 4
AR 90
DI 10.3847/0004-6256/151/4/90
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DL4LV
UT WOS:000375609100003
ER
PT J
AU Bohle, S
Montano, HSP
Bille, M
Turnbull, D
AF Bohle, Shannon
Montano, H. Saul Perez
Bille, Matt
Turnbull, Doug
TI Evolution of soil on Mars
SO ASTRONOMY & GEOPHYSICS
LA English
DT Article
ID LIFE
C1 [Bohle, Shannon] NASA, Jet Prop Lab, Neil Armstrong Lib & Arch, Aurora, CO USA.
[Montano, H. Saul Perez] NASA Ames, Aurora, CO USA.
RP Bohle, S (reprint author), NASA, Jet Prop Lab, Neil Armstrong Lib & Arch, Aurora, CO USA.
NR 36
TC 0
Z9 0
U1 4
U2 8
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 1366-8781
EI 1468-4004
J9 ASTRON GEOPHYS
JI Astron. Geophys.
PD APR
PY 2016
VL 57
IS 2
BP 18
EP 23
PG 6
WC Astronomy & Astrophysics; Geochemistry & Geophysics
SC Astronomy & Astrophysics; Geochemistry & Geophysics
GA DJ8QE
UT WOS:000374476300019
ER
PT J
AU Chen, Y
Morton, DC
Andela, N
Giglio, L
Randerson, JT
AF Chen, Yang
Morton, Douglas C.
Andela, Niels
Giglio, Louis
Randerson, James T.
TI How much global burned area can be forecast on seasonal time scales
using sea surface temperatures?
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE biomass burning; teleconnection; seasonal outlook; mitigation
ID BIOMASS BURNING EMISSIONS; FIRE DANGER FORECASTS; INTERANNUAL
VARIABILITY; SOUTHEAST-ASIA; EL-NINO; STATISTICAL-MODEL; WILDFIRE
ACTIVITY; DROUGHT; SEVERITY; CLIMATE
AB Large-scale sea surface temperature (SST) patterns influence the interannual variability of burned area in many regions by means of climate controls on fuel continuity, amount, and moisture content. Some of the variability in burned area is predictable on seasonal timescales because fuel characteristics respond to the cumulative effects of climate prior to the onset of the fire season. Here we systematically evaluated the degree to which annual burned area from the Global Fire Emissions Database version 4 with small fires (GFED4s) can be predicted using SSTs from 14 different ocean regions. We found that about 48% of global burned area can be forecast with a correlation coefficient that is significant at a p < 0.01 level using a single ocean climate index (OCI) 3 or more months prior to the month of peak burning. Continental regions where burned area had a higher degree of predictability included equatorial Asia, where 92% of the burned area exceeded the correlation threshold, and Central America, where 86% of the burned area exceeded this threshold. Pacific Ocean indices describing the El Nino-Southern Oscillation were more important than indices from other ocean basins, accounting for about 1/3 of the total predictable global burned area. A model that combined two indices from different oceans considerably improved model performance, suggesting that fires in many regions respond to forcing from more than one ocean basin. Using OCI-burned area relationships and a clustering algorithm, we identified 12 hotspot regions in which fires had a consistent response to SST patterns. Annual burned area in these regions can be predicted with moderate confidence levels, suggesting operational forecasts may be possible with the aim of improving ecosystem management.
C1 [Chen, Yang; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Morton, Douglas C.; Andela, Niels] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Giglio, Louis] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
RP Chen, Y (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM yang.chen@uci.edu
RI Morton, Douglas/D-5044-2012
FU Gordon and Betty Moore Foundation [GBMF3269]; NASA's Interdisciplinary
Research in Earth Science Program
FX This work would not have been possible without near real-time access to
ocean climate indices provided by NOAA's State of the Ocean climate
program (http://stateoftheocean.osmc.noaa.gov) and past NASA investment
in the Earth Observing System and the Global Fire Emissions Database.
This research was supported by a grant to Randerson from the Gordon and
Betty Moore Foundation (GBMF3269) and to Morton from NASA's
Interdisciplinary Research in Earth Science Program.
NR 59
TC 2
Z9 2
U1 6
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD APR
PY 2016
VL 11
IS 4
AR 045001
DI 10.1088/1748-9326/11/4/045001
PG 13
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DL6JZ
UT WOS:000375746800029
ER
PT J
AU Cook, J
Oreskes, N
Doran, PT
Anderegg, WRL
Verheggen, B
Maibach, EW
Carlton, JS
Lewandowsky, S
Skuce, AG
Green, SA
Nuccitelli, D
Jacobs, P
Richardson, M
Winkler, B
Painting, R
Rice, K
AF Cook, John
Oreskes, Naomi
Doran, Peter T.
Anderegg, William R. L.
Verheggen, Bart
Maibach, Ed W.
Carlton, J. Stuart
Lewandowsky, Stephan
Skuce, Andrew G.
Green, Sarah A.
Nuccitelli, Dana
Jacobs, Peter
Richardson, Mark
Winkler, Barbel
Painting, Rob
Rice, Ken
TI Consensus on consensus: a synthesis of consensus estimates on
human-caused global warming
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Editorial Material
DE scientific consensus; climate change; anthropogenic global warming
ID CLIMATE-CHANGE; SCIENTIFIC AGREEMENT; SUPPORT; VIEWS
AB The consensus that humans are causing recent global warming is shared by 90%-100% of publishing climate scientists according to six independent studies by co-authors of this paper. Those results are consistent with the 97% consensus reported by Cook et al (Environ. Res. Lett. 8 024024) based on 11 944 abstracts of research papers, of which 4014 took a position on the cause of recent global warming. A survey of authors of those papers (N = 2412 papers) also supported a 97% consensus. Tol (2016 Environ. Res. Lett. 11 048001) comes to a different conclusion using results from surveys of nonexperts such as economic geologists and a self-selected group of those who reject the consensus. We demonstrate that this outcome is not unexpected because the level of consensus correlates with expertise in climate science. At one point, Tol also reduces the apparent consensus by assuming that abstracts that do not explicitly state the cause of global warming ('no position') represent nonendorsement, an approach that if applied elsewhere would reject consensus on well-established theories such as plate tectonics. We examine the available studies and conclude that the finding of 97% consensus in published climate research is robust and consistent with other surveys of climate scientists and peer-reviewed studies.
C1 [Cook, John] Univ Queensland, Global Change Inst, Brisbane, Qld 4072, Australia.
[Cook, John; Lewandowsky, Stephan] Univ Western Australia, Sch Psychol, Nedlands, WA 6009, Australia.
[Cook, John; Skuce, Andrew G.; Nuccitelli, Dana; Winkler, Barbel; Painting, Rob] Skept Sci, Brisbane, Qld, Australia.
[Oreskes, Naomi] Harvard Univ, Dept Hist Sci, Cambridge, MA 02138 USA.
[Doran, Peter T.] Louisiana State Univ, Geol & Geophys, Baton Rouge, LA 70803 USA.
[Anderegg, William R. L.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
[Anderegg, William R. L.] Princeton Univ, Princeton Environm Inst, Princeton, NJ 08544 USA.
[Verheggen, Bart] Amsterdam Univ Coll, Amsterdam, Netherlands.
[Maibach, Ed W.; Jacobs, Peter] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA.
[Carlton, J. Stuart] Texas A&M Univ, Texas Sea Grant Coll Program, College Stn, TX USA.
[Lewandowsky, Stephan] Univ Bristol, Bristol BS8 1TH, Avon, England.
[Skuce, Andrew G.] Salt Spring Consulting Ltd, Salt Spring Isl, BC, Canada.
[Green, Sarah A.] Michigan Technol Univ, Dept Chem, Houghton, MI 49931 USA.
[Richardson, Mark] Univ Reading, Reading RG6 2AH, Berks, England.
[Richardson, Mark] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Rice, Ken] Univ Edinburgh, Inst Astron, Edinburgh, Midlothian, Scotland.
RP Cook, J (reprint author), Univ Queensland, Global Change Inst, Brisbane, Qld 4072, Australia.; Cook, J (reprint author), Univ Western Australia, Sch Psychol, Nedlands, WA 6009, Australia.; Cook, J (reprint author), Skept Sci, Brisbane, Qld, Australia.
EM j.cook3@uq.edu.au
RI Rice, Ken/H-5084-2011;
OI Rice, Ken/0000-0002-6379-9185; Lewandowsky, Stephan/0000-0003-1655-2013;
Green, Sarah/0000-0002-8094-433X; Richardson, Mark/0000-0001-7063-631X;
Jacobs, Peter/0000-0002-6951-7126
NR 36
TC 10
Z9 10
U1 36
U2 55
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD APR
PY 2016
VL 11
IS 4
AR 048002
DI 10.1088/1748-9326/11/4/048002
PG 7
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DL6JZ
UT WOS:000375746800038
ER
PT J
AU Foster, LM
Bearup, LA
Molotch, NP
Brooks, PD
Maxwell, RM
AF Foster, Lauren M.
Bearup, Lindsay A.
Molotch, Noah P.
Brooks, Paul D.
Maxwell, Reed M.
TI Energy budget increases reduce mean streamflow more than snow-rain
transitions: using integrated modeling to isolate climate change impacts
on Rocky Mountain hydrology
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE Rocky Mountains; climate change; integrated modeling; snow to rain
transitions; energy budget; hydrology; precipitation phase
ID WESTERN UNITED-STATES; WATER-GROUNDWATER INTERACTIONS; COLORADO
RIVER-BASIN; SURFACE-WATER; AVAILABILITY; SENSITIVITY; TRENDS;
VARIABILITY; SIMULATION; RESOURCES
AB In snow-dominated mountain regions, a warming climate is expected to alter two drivers of hydrology: (1) decrease the fraction of precipitation falling as snow; and (2) increase surface energy available to drive evapotranspiration. This study uses a novel integrated modeling approach to explicitly separate energy budget increases via warming from precipitation phase transitions from snow to rain in two mountain headwaters transects of the central Rocky Mountains. Both phase transitions and energy increases had significant, though unique, impacts on semi-arid mountain hydrology in our simulations. A complete shift in precipitation from snow to rain reduced streamflow between 11% and 18%, while 4 degrees C of uniform warming reduced streamflow between 19% and 23%, suggesting that changes in energy-driven evaporative loss, between 27% and 29% for these uniform warming scenarios, may be the dominant driver of annual mean streamflow in a warming climate. Phase changes induced a flashier system, making water availability more susceptible to precipitation variability and eliminating the runoff signature characteristic of snowmelt-dominated systems. The impact of a phase change on mean streamflow was reduced as aridity increased from west to east of the continental divide.
C1 [Foster, Lauren M.; Bearup, Lindsay A.; Maxwell, Reed M.] Colorado Sch Mines, Dept Geol Engn, Golden, CO 80401 USA.
[Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Brooks, Paul D.] Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA.
RP Foster, LM; Maxwell, RM (reprint author), Colorado Sch Mines, Dept Geol Engn, Golden, CO 80401 USA.
EM lfoster@mines.edu; rmaxwell@mines.edu
RI Bearup, Lindsay/J-1923-2016; Molotch, Noah/C-8576-2009
OI Bearup, Lindsay/0000-0003-2339-1983;
FU National Science Foundation IGERT (Integrated Graduate Education and
Research Traineeship) [DGE-1069333]; Colorado School of Mines
FX This study was funded by a National Science Foundation IGERT (Integrated
Graduate Education and Research Traineeship) under award DGE-1069333 (to
L Foster and R Maxwell) and Dean's Fellowship from the Colorado School
of Mines (to L Foster).
NR 49
TC 1
Z9 1
U1 9
U2 15
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD APR
PY 2016
VL 11
IS 4
AR 044015
DI 10.1088/1748-9326/11/4/044015
PG 10
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DL6JZ
UT WOS:000375746800019
ER
PT J
AU Garrett, RD
Carlson, KM
Rueda, X
Noojipady, P
AF Garrett, Rachael D.
Carlson, Kimberly M.
Rueda, Ximena
Noojipady, Praveen
TI Assessing the potential additionality of certification by the Round
table on Responsible Soybeans and the Roundtable on Sustainable Palm Oil
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE agricultural expansion; environmental governance; tropical
deforestation; South America; Southeast Asia; oilseeds
ID BRAZILIAN AMAZON; ENVIRONMENTAL-PROTECTION; SMALLHOLDER FARMERS; FAIR
TRADE; LAND-USE; GOVERNANCE; DEFORESTATION; CONSERVATION; AGRICULTURE;
STANDARDS
AB Multi-stakeholder roundtables offering certification programs are promising voluntary governance mechanisms to address sustainability issues associated with international agricultural supply chains. Yet, little is known about whether roundtable certifications confer additionality, the benefits of certification beyond what would be expected from policies and practices currently in place. Here, we examine the potential additionality of the Round table on Responsible Soybeans (RTRS) and the Roundtable on Sustainable PalmOil (RSPO) in mitigating conversion of native vegetation to cropland. We develop a metric of additionality based on business as usual land cover change dynamics and roundtable standard stringency relative to existing policies. We apply this metric to all countries with RTRS (n = 8) and RSPO(n = 12) certified production in 2013-2014, as well as countries that have no certified production but are among the top ten global producers in terms of soy (n = 2) and oil palm (N = 2). We find RSPO and RTRS both have substantially higher levels of stringency than existing national policies except in Brazil and Uruguay. In regions where these certification standards are adopted, the mean estimated rate of tree cover conversion to the target crop is similar for both standards. RTRS has higher mean relative stringency than the RSPO, yet RSPO countries have slightly higher enforcement levels. Therefore, mean potential additionality of RTRS and RSPO is similar across regions. Notably, countries with the highest levels of additionality have some adoption. However, with extremely low adoption rates (0.41% of 2014 global harvested area), RTRS likely has lower impact than RSPO (14%). Likemost certification programs, neither roundtable is effectively targeting smallholder producers. To improve natural ecosystem protection, roundtables could target adoption to regions with low levels of environmental governance and high rates of forest-to-cropland conversion.
C1 [Garrett, Rachael D.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Carlson, Kimberly M.] Univ Hawaii Manoa, Dept Nat Resources & Environm Management, Honolulu, HI 96822 USA.
[Carlson, Kimberly M.] Univ Minnesota, Inst Environm, St Paul, MN 55108 USA.
[Rueda, Ximena] Univ Los Andes, Sch Management, Bogota, Colombia.
[Noojipady, Praveen] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD USA.
[Noojipady, Praveen] Natl Wildlife Federat, Natl Advocacy Ctr, Washington, DC USA.
[Noojipady, Praveen] Univ Maryland, College Pk, MD 20742 USA.
RP Garrett, RD (reprint author), Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
EM rgarr@bu.edu
OI Garrett, Rachael/0000-0002-6171-263X; Rueda, Ximena/0000-0002-5991-4048
FU Gordon and Betty Moore Foundation; General Mills; Mosaic; Cargill;
Kellogg's; Mars; PepsiCo; Giorgio Ruffolo Fellowship in Sustainability
Science at Harvard University; National Science Foundation Science,
Engineering, and Education for Sustainability Program [256, 940];
Italy's Ministry for Environment, Land and Sea; National Academies Keck
Futures Initiative
FX We thank Eric Lambin and four anonymous reviewers for their very helpful
feedback on this manuscript. The Gordon and Betty Moore Foundation
provided primary research funding to the Institute on the Environment at
the University of Minnesota for KMC. Contributions by General Mills,
Mosaic, Cargill, Kellogg's, Mars, and PepsiCo supported stakeholder
outreach and public engagement. RDG was funded by the Giorgio Ruffolo
Fellowship in Sustainability Science at Harvard University and the
National Science Foundation Science, Engineering, and Education for
Sustainability Program (Grant #256, 940). Support from Italy's Ministry
for Environment, Land and Sea, as well as the National Academies Keck
Futures Initiative, is gratefully acknowledged. The funders had no role
in study design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 70
TC 4
Z9 4
U1 18
U2 31
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD APR
PY 2016
VL 11
IS 4
AR 045003
DI 10.1088/1748-9326/11/4/045003
PG 17
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DL6JZ
UT WOS:000375746800031
ER
PT J
AU Kharuk, VI
Shushpanov, AS
Im, ST
Ranson, KJ
AF Kharuk, Viacheslav I.
Shushpanov, Alexandr S.
Im, Sergei T.
Ranson, Kenneth J.
TI Climate-induced landsliding within the larch dominant permafrost zone of
central Siberia
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE permafrost in Siberia; larch forests; landslides; GRACE; landslides
hazard; permafrost melting; landslides in permafrost
ID GRACE; MODEL; GIS
AB Climate impact on landslide occurrence and spatial patterns were analyzed within the larch-dominant communities associated with continuous permafrost areas of central Siberia. We used high resolution satellite imagery (i.e. QuickBird, WorldView) to identify landslide scars over an area of 62 000 km(2). Landslide occurrence was analyzed with respect to climate variables (air temperature, precipitation, drought index SPEI), and Gravity Recovery and Climate Experiment satellite derived equivalent of water thickness anomalies (EWTA). Landslides were found only on southward facing slopes, and the occurrence of landslides increased exponentially with increasing slope steepness. Lengths of landslides correlated positively with slope steepness. The observed upper elevation limit of landslides tended to coincide with the tree line. Observations revealed landslides occurrence was also found to be strongly correlated with August precipitation (r = 0.81) and drought index (r = 0.7), with June-July-August soil water anomalies (i.e., EWTA, r = 0.68-0.7), and number of thawing days (i.e., a number of days with t(max) > 0 degrees C; r = 0.67). A significant increase in the variance of soil water anomalies was observed, indicating that occurrence of landslides may increase even with a stable mean precipitation level. The key-findings of this study are (1) landslides occurrence increased within the permafrost zone of central Siberia in the beginning of the 21st century; (2) the main cause of increased landslides occurrence are extremes in precipitation and soil water anomalies; and (3) landslides occurrence are strongly dependent on relief features such as southward facing steep slopes.
C1 [Kharuk, Viacheslav I.; Shushpanov, Alexandr S.; Im, Sergei T.] Sukachev Forest Inst, Krasnoyarsk 660036, Russia.
[Kharuk, Viacheslav I.; Im, Sergei T.] Siberian Fed Univ, Krasnoyarsk 660041, Russia.
[Im, Sergei T.] Siberian State Aerosp Univ, Krasnoyarsk 660014, Russia.
[Ranson, Kenneth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kharuk, VI (reprint author), Sukachev Forest Inst, Krasnoyarsk 660036, Russia.; Kharuk, VI (reprint author), Siberian Fed Univ, Krasnoyarsk 660041, Russia.
EM kharuk@ksc.krasn.ru; alexandr01061987@gmail.com; stim@ksc.krasn.ru;
kenneth.j.ranson@nasa.gov
RI Im, Sergei/J-2736-2016
OI Im, Sergei/0000-0002-5794-7938
FU Russian Science Foundation [14-24-00112]; NASA's Terrestrial Ecology
program; NASA MEaSUREs Program
FX Russian Science Foundation (grant #14-24-00112) primarily supported this
research. Additional support for K J Ranson by NASA's Terrestrial
Ecology program. GRACE land data were preprocessed by Sean Swenson,
supported by the NASA MEaSUREs Program, and are available at
http://grace.jpl.nasa.gov. DigitalGlobe data were provided by NASA's NGA
Commercial Archive Data (cad4nasa.gsfc.nasa.gov) under the National
Geospatial-Intelligence Agency's NextView license agreement.
NR 42
TC 0
Z9 0
U1 3
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD APR
PY 2016
VL 11
IS 4
AR 045004
DI 10.1088/1748-9326/11/4/045004
PG 20
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DL6JZ
UT WOS:000375746800032
ER
PT J
AU Yasumiishi, EM
Criddle, KR
Helle, JH
Hillgruber, N
Mueter, FJ
AF Yasumiishi, Ellen M.
Criddle, Keith R.
Helle, John H.
Hillgruber, Nicola
Mueter, Franz J.
TI Effect of population abundance and climate on the growth of 2
populations of chum salmon (Oncorhynchus keta) in the eastern North
Pacific Ocean
SO FISHERY BULLETIN
LA English
DT Article
ID PINK SALMON; SOCKEYE-SALMON; BERING-SEA; BODY-SIZE; HATCHERY PROGRAMS;
BRITISH-COLUMBIA; MARINE SURVIVAL; ALASKA; RIVER; GORBUSCHA
AB Seasonal and annual marine growth of chum salmon (Oncorhynchus keta) from Fish Creek, Alaska, during 1972-2004 and from Quilcene River, Washington., during 1973-2004 were examined in relation to abundances of chum salmon and pink salmon (O. gorbuscha) and climate indices from that period. Pink salmon abundance indices were included in the analysis because of evidence for density-dependent effects on chum salmon growth and survival. In linear regression models, growth was negatively related to abundance of chum salmon or to the combined abundance of pink and chum salmon during the middle juvenile (July-Sept), 1st immature, 2nd immature, and maturing stages for the Fish Creek chum salmon and the 1st immature, 2nd immature, and maturing stages for Quilcene River chum salmon, indicating possible density-dependent effects on growth. Mid-juvenile and maturing growth models for the Fish Creek chum salmon and the maturing growth model for Quilcene River chum salmon performed well in model validation, when model predictions were tested against 20% of the data that were not used for model specification, and provided insight into the effects of climate and abundance on growth of chum salmon from 1972 to 2004.
C1 [Yasumiishi, Ellen M.; Criddle, Keith R.; Helle, John H.; Hillgruber, Nicola; Mueter, Franz J.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, 17101 Point Lena Loop Rd, Juneau, AK 99801 USA.
[Yasumiishi, Ellen M.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv,Ted Stevens Marine Res, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
[Helle, John H.] 2427 ODay Dr, Juneau, AK 99801 USA.
[Hillgruber, Nicola] Thunen Inst Fisheries Ecol, Wulfsdorfer Weg 204, D-22926 Ahrensburg, Germany.
RP Yasumiishi, EM (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, 17101 Point Lena Loop Rd, Juneau, AK 99801 USA.; Yasumiishi, EM (reprint author), NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv,Ted Stevens Marine Res, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM ellen.yasumiishi@noaa.gov
FU Alaska Fisheries Science Center in Juneau, Alaska; Advanced Studies
Program, Professional Development program of the National Oceanic and
Atmospheric Administration
FX Funding and support for this project was received from the Alaska
Fisheries Science Center in Juneau, Alaska and the Advanced Studies
Program, Professional Development program of the National Oceanic and
Atmospheric Administration. We greatly appreciate the assistance of all
the people that helped with field collection throughout the years and
the assistance of the Alaska Department of Fish and Game in Ketchikan
and the U.S. Fish and Wildlife Service at the Quilcene National Fish
Hatchery in Quilcene, Washington. We appreciate the constructive
comments from Phil Mundy, Ed Farley, and Lisa Eisner. We also thank the
anonymous reviewers for their thoughtful suggestions that greatly
improved the manuscript.
NR 74
TC 0
Z9 0
U1 5
U2 12
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
EI 1937-4518
J9 FISH B-NOAA
JI Fish. Bull.
PD APR
PY 2016
VL 114
IS 2
BP 203
EP 219
DI 10.7755/FB.114.2.7
PG 17
WC Fisheries
SC Fisheries
GA DK2DF
UT WOS:000374724100007
ER
PT J
AU Weijerman, M
Williams, I
Gutierrez, J
Grafeld, S
Tibbatts, B
Davis, G
AF Weijerman, Mariska
Williams, Ivor
Gutierrez, Jay
Grafeld, Shanna
Tibbatts, Brent
Davis, Gerry
TI Trends in biomass of coral reef fishes, derived from shore-based creel
surveys in Guam
SO FISHERY BULLETIN
LA English
DT Article
ID MANAGEMENT; PACIFIC; RESILIENCE; MICRONESIA; ECOSYSTEMS; ISLANDS; TRADE
AB Coral reef fisheries have a cultural, economic, and ecological importance and sustain the societal well-being of many coastal communities. However, the complexities of the multigear, multispecies fisheries that target coral reef species pose challenges for fisheries management. We focus on the Guam shore-based coral reef fishery 1) to evaluate the characteristics of the past and recent fishery in terms of catch composition and effort per gear type and 2) to reconstruct the reef-fish population in shallow (depths <= 30 m) water during 1985-2012. To accomplish this, we used the results from a detailed creel survey conducted by the Guam Division of Aquatic and Wildlife Resources. The total estimated effort has stayed more or less stable; however, the estimated total catch has dropped from an annual mean of 100 metric tons (t) during the period 1985-1990 to 37 t during the period 2007-2012. Catch per unit of effort (CPUE) declined for most gear types between the 2 time periods. Reconstruction. of historical targeted fish biomass, based on CPUE, showed a general decrease in biomass from 1985 to 2012. Biomass quickly dropped to about half of the 1985 values, then leveled off for a decade before declining again beginning in 2003 and continuing through 2012.
C1 [Weijerman, Mariska] Univ Hawaii Manoa, Joint Inst Marine & Atmospher Res, Sch Ocean & Earth Sci & Technol, Marine Sci Bldg 312,1000 Pope Rd, Honolulu, HI 96822 USA.
[Weijerman, Mariska] Wageningen Univ, Environm Syst Anal Grp, POB 47, NL-6700 AA Wageningen, Netherlands.
[Williams, Ivor] NOAA, Coral Reef Ecosyst Program, Pacific Isl Fisheries Sci Ctr, Natl Mariner Fisheries Serv, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
[Gutierrez, Jay; Tibbatts, Brent] Guam Dept Agr, Div Aquat & Wildlife Resources, 163 Dairy Rd, Mangilao, GU 96913 USA.
[Grafeld, Shanna] Univ Hawaii Manoa, Dept Nat Resources & Environm Management, 1910 East West Rd,Sherman Lab 101, Honolulu, HI 96822 USA.
[Davis, Gerry] NOAA, Habitat Conservat Div, Pacific Isl Reg Off, Natl Marine Fisheries Serv, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
RP Weijerman, M (reprint author), Univ Hawaii Manoa, Joint Inst Marine & Atmospher Res, Sch Ocean & Earth Sci & Technol, Marine Sci Bldg 312,1000 Pope Rd, Honolulu, HI 96822 USA.; Weijerman, M (reprint author), Wageningen Univ, Environm Syst Anal Grp, POB 47, NL-6700 AA Wageningen, Netherlands.
EM mariska.weijerman@noaa.gov
FU NOAA Coral Reef Conservation Program
FX Funding for the senior author and S. Grafeld was obtained from the NOAA
Coral Reef Conservation Program. We would like to acknowledge the staff
at the Division of Aquatic and Wildlife Resources, Guam Department of
Agriculture, for data collection and the following people at the NOAA
Pacific Islands Fisheries Science Center: K. Low, M. Quack, and P. Tao
for extracting and helping to interpret data, M. Nadon for advice on
data analyses, and C. Boggs and J. Wetherall for their valuable comments
on the draft manuscript.
NR 40
TC 0
Z9 0
U1 2
U2 5
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
EI 1937-4518
J9 FISH B-NOAA
JI Fish. Bull.
PD APR
PY 2016
VL 114
IS 2
BP 237
EP 256
DI 10.7755/FB.114.2.9
PG 20
WC Fisheries
SC Fisheries
GA DK2DF
UT WOS:000374724100009
ER
PT J
AU Xu, XL
Derksen, C
Yueh, SH
Dunbar, RS
Colliander, A
AF Xu, Xiaolan
Derksen, Chris
Yueh, Simon H.
Dunbar, Roy Scott
Colliander, Andreas
TI Freeze/Thaw Detection and Validation Using Aquarius' L-Band
Backscattering Data
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Environmental monitoring; land surface; radar remote sensing
ID NON-FROZEN SEASONS; VEGETATION GROWTH; SCATTEROMETER DATA; SOIL
PROCESSES; SPRING THAW; BOREAL; CYCLES; RADAR; SENSITIVITY; LANDSCAPE
AB The seasonal cycle of landscape freeze/thaw (FT) state acrossmid-to high latitudes influences critical processes such as the land surface energy balance, carbon cycle dynamics related to vegetation growth, and hydrological partitioning between surface runoff and infiltration. In this paper, we produce the first daily FT classification for the 2011-2014 period based on L-band radar measurements from Aquarius. The radar FT algorithm used in this paper is based on a seasonal threshold approach, which is also the baseline algorithm applied to higher-resolution (3 km) radar measurements from NASA's Soil Moisture Active/Passive (SMAP) mission (Launched January 31, 2015). The lower frequency (L-band) radar backscatter measurements from Aquarius provide enhanced sensitivity to FT conditions in vegetation canopy, snow and surface soil layers, although the relative radar penetration depth and sensitivity of the FT signal to these landscape elements will vary according to surface moisture and vegetation biomass conditions, and underlying land cover and terrain heterogeneity [1], [2]. Evaluation of the seasonal threshold FT algorithm using Aquarius was performed using surface air and soil temperatures from selected stations in the Snow Telemetry (SnoTel) network. Analysis identified good agreement during the fall freezeup period with flag agreement exceeding the 80% SMAP accuracy target when summarized on a monthly basis. Disagreement was greater during the spring thaw transition due in part to uncertainty in characterizing thaw from in situ measurements. Unlike the fall season, stronger agreement in the spring was identified when the reference state was characterized with air temperature compared to soil temperature.
C1 [Xu, Xiaolan; Yueh, Simon H.; Dunbar, Roy Scott; Colliander, Andreas] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Derksen, Chris] Environm Canada, Ottawa, ON, Canada.
RP Xu, XL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM xiaolan.xu@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology under
National Aeronautics and Space Administration
FX This work was supported by the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. The Group for Level 2 Aquarius backscattering
data were obtained from the NASA EOSDIS Physical Oceanography
Distributed Active Archive Center (PO.DAAC) at the Jet Propulsion
Laboratory, Pasadena, CA.
NR 33
TC 1
Z9 1
U1 4
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2016
VL 9
IS 4
BP 1370
EP 1381
DI 10.1109/JSTARS.2016.2519347
PG 12
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DL8DA
UT WOS:000375868800005
ER
PT J
AU Liao, TH
Kim, SB
Tan, SR
Tsang, L
Su, CX
Jackson, TJ
AF Liao, Tien-Hao
Kim, Seung-Bum
Tan, Shurun
Tsang, Leung
Su, Chenxin
Jackson, Thomas J.
TI Multiple Scattering Effects With Cyclical Correction in Active Remote
Sensing of Vegetated Surface Using Vector Radiative Transfer Theory
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Backscattering enhancement; cyclical correction; multiple scattering
effects; remote sensing; soil moisture; vector radiative transfer
ID BACKSCATTERING ENHANCEMENT; SOIL; MODEL; TERRAIN; RADAR; LAYER
AB The energy transport in a vegetated (corn) surface layer is examined by solving the vector radiative transfer equation using a numerical iterative approach. This approach allows a higher order that includes the multiple scattering effects. Multiple scattering effects are important when the optical thickness and scattering albedo of the vegetation layer are large. When both the albedo and the optical thickness exceed 0.4, higher orders contribute significantly (e.g., vertical polarization at L-band). The approach is applied to vegetated surfaces using typical crop structure for backscattering from L-band to Ku-band. For corn fields at L-band, multiple scattering effects are more important for vertical scattered wave with vertical incidence (VV). For example, when vegetation water content (VWC) is 3kg/m(2), the deviation between first order and multiple scattering for corn field for VV could be 3.5 dB while 0.7 dB for horizontal scattered wave with horizontal incidence (HH). The iterative approach also allows the separation of the contribution to backscattering from each scattering order and scattering mechanism. Each scattering mechanism is associated with a unique scattering path. By examining the duality of the paths, we are able to identify the cyclical terms with existence of a reflective boundary. The cyclical correction to the backscattering accounts for backscattering enhancement effects on the copolarization by a factor of two. The approach is validated against the SMAPVEX12 L-band corn dataset over the entire crop growth and large soil moisture variations. The model prediction matches the observation with 1.93 and 1.46 dB root-mean-square error (RMSE) for VV and HH, respectively, while correlations are 0.67 and 0.88, respectively. Time-series retrieval is also applied successfully for both soil moisture and VWC with 0.06 cm(3)/cm(3) and 0.44 kg/m(2) RMSE, respectively, while correlations are 0.7 and 0.92, respectively. For large VWC, this approach corrects the underestimated backscatters in the single scattering caused by large attenuation.
C1 [Liao, Tien-Hao; Tan, Shurun; Tsang, Leung] Univ Michigan, Dept Elect Engn & Comp Sci, Ann Arbor, MI 48109 USA.
[Kim, Seung-Bum] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Su, Chenxin] Univ Washington, Elect Engn, Seattle, WA 98195 USA.
[Jackson, Thomas J.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA.
RP Liao, TH (reprint author), Univ Michigan, Dept Elect Engn & Comp Sci, Ann Arbor, MI 48109 USA.
EM thliao@uw.edu
FU NASA SMAP; National Aeronautics and Space Administration
FX The authors would like to thank NASA SMAP project to support the work
and the SMAPVEX12 team to provide the measurement data. The research
described in this publication was carried out in part at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. Surface
scattering results from NMM3D were computed using NSF XSEDE facility.
NR 24
TC 1
Z9 1
U1 1
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2016
VL 9
IS 4
BP 1414
EP 1429
DI 10.1109/JSTARS.2015.2505638
PG 16
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DL8DA
UT WOS:000375868800008
ER
PT J
AU Parveg, D
Varonen, M
Kangaslahti, P
Safaripour, A
Hajimiri, A
Tikka, T
Gaier, T
Halonen, KAI
AF Parveg, Dristy
Varonen, Mikko
Kangaslahti, Pekka
Safaripour, Amirreza
Hajimiri, Ali
Tikka, Tero
Gaier, Todd
Halonen, Kari A. I.
TI CMOS I/Q Subharmonic Mixer for Millimeter-Wave Atmospheric Remote
Sensing
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE CMOS integrated circuit; millimeter-wave integrated circuit; mixers;
MMICs; remote sensing
ID TRANSCEIVER
AB A compact second harmonic 180 GHz I/Q balanced resistive mixer is realized in a 32-nm SOI CMOS technology for atmospheric remote sensing applications. The MMIC further includes two on-chip IF amplifiers at the mixer's I and Q channels. A conversion gain of +8 dB is achieved with 74 mW of dc power consumption using a 1.2 V supply. The measured IF frequency range is from 1 to 10 GHz. The mixer achieves a 20 dB image-rejection (IR) ratio with an LO input power of +4 dBm. The chip size is 0.75 mm(2) including probing pads.
C1 [Parveg, Dristy; Varonen, Mikko; Tikka, Tero; Halonen, Kari A. I.] Aalto Univ, Dept Micro & Nanosci, Espoo 02150, Finland.
[Kangaslahti, Pekka; Gaier, Todd] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Safaripour, Amirreza; Hajimiri, Ali] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
RP Parveg, D (reprint author), Aalto Univ, Dept Micro & Nanosci, Espoo 02150, Finland.
EM dristy.parveg@aalto.fi
FU Academy of Finland; Jet Propulsion Laboratory (JPL), California
Institute of Technology, under National Aeronautics and Space
Administration (NASA)
FX This work was supported by the Academy of Finland through the FAMOS
project and Postdoctoral research post and in part by the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under a contract
with the National Aeronautics and Space Administration (NASA).
NR 11
TC 0
Z9 0
U1 1
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1531-1309
EI 1558-1764
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD APR
PY 2016
VL 26
IS 4
BP 285
EP 287
DI 10.1109/LMWC.2016.2537786
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA DJ9VS
UT WOS:000374561900021
ER
PT J
AU Zhang, XY
Zhang, QY
AF Zhang, Xiaoyang
Zhang, Qingyuan
TI Monitoring interannual variation in global crop yield using long-term
AVHRR and MODIS observations
SO ISPRS JOURNAL OF PHOTOGRAMMETRY AND REMOTE SENSING
LA English
DT Article
DE Global crop yield; Crop phenology; Crop greenness; Long-term satellite
observations
ID VEGETATION HEALTH INDEXES; NET PRIMARY PRODUCTIVITY; GROSS PRIMARY
PRODUCTION; LAND-SURFACE PHENOLOGY; WINTER-WHEAT YIELD; UNITED-STATES;
TIME-SERIES; NDVI DATA; COVER PRODUCTS; BURKINA-FASO
AB Advanced Very High Resolution Radiometer (AVHRR) and Moderate Resolution Imaging Spectroradiometer (MODIS) data have been extensively applied for crop yield prediction because of their daily temporal resolution and a global coverage. This study investigated global crop yield using daily two band Enhanced Vegetation Index (EVI2) derived from AVHRR (1981-1999) and MODIS (2000-2013) observations at a spatial resolution of 0.05 degrees (similar to 5 km). Specifically, EVI2 temporal trajectory of crop growth was simulated using a hybrid piecewise logistic model (HPLM) for individual pixels, which was used to detect crop phenological metrics. The derived crop phenology was then applied to calculate crop greenness defined as EVI2 amplitude and EVI2 integration during annual crop growing seasons, which was further aggregated for croplands in each country, respectively. The interannual variations in EVI2 amplitude and EVI2 integration were combined to correlate to the variation in cereal yield from 1982-2012 for individual countries using a stepwise regression model, respectively. The results show that the confidence level of the established regression models was higher than 90% (P value < 0.1) in most countries in the northern hemisphere although it was relatively poor in the southern hemisphere (mainly in Africa). The error in the yield predication was relatively smaller in America, Europe and East Asia than that in Africa. In the 10 countries with largest cereal production across the world, the prediction error was less than 9% during past three decades. This suggests that crop phenology-controlled greenness from coarse resolution satellite data has the capability of predicting national crop yield across the world, which could provide timely and reliable crop information for global agricultural trade and policymakers. (C) 2016 International Society for Photogrammetry and Remote Sensing, Inc. (ISPRS). Published by Elsevier B.V. All rights reserved.
C1 [Zhang, Xiaoyang] S Dakota State Univ, Dept Geog, GSCE, 1021 Medary Ave,Wecota Hall 506B, Brookings, SD 57007 USA.
[Zhang, Qingyuan] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Zhang, Qingyuan] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 661, Greenbelt, MD 20771 USA.
RP Zhang, XY (reprint author), S Dakota State Univ, Dept Geog, GSCE, 1021 Medary Ave,Wecota Hall 506B, Brookings, SD 57007 USA.
EM xiaoyang.zhang@sdstate.edu
OI Zhang, Xiaoyang/0000-0001-8456-0547
FU NASA [NNX15AB96A]; NOAA [JPSS_PGRR2_14]
FX This work was supported by NASA contracts NNX15AB96A and NOAA contract
JPSS_PGRR2_14. The reviewers are thanked for the constructive comments
during the review process of the manuscript.
NR 90
TC 1
Z9 1
U1 9
U2 19
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0924-2716
EI 1872-8235
J9 ISPRS J PHOTOGRAMM
JI ISPRS-J. Photogramm. Remote Sens.
PD APR
PY 2016
VL 114
BP 191
EP 205
DI 10.1016/j.isprsjprs.2016.02.010
PG 15
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
Photographic Technology
GA DK1XG
UT WOS:000374707800017
ER
PT J
AU Oh, D
Hashimoto, J
Tamura, M
Wisniewski, J
Akiyama, E
Currie, T
Mayama, S
Takami, M
Thalmann, C
Kudo, T
Kusakabe, N
Abe, L
Brandner, W
Brandt, TD
Carson, JC
Egner, S
Feldt, M
Goto, M
Grady, CA
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, SS
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, GR
Kuzuhara, M
Kwon, J
Matsuo, T
McElwain, MW
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, YH
Takato, N
Terada, H
Turner, EL
Watanabe, M
Yamada, T
Takami, H
Usuda, T
AF Oh, Daehyeon
Hashimoto, Jun
Tamura, Motohide
Wisniewski, John
Akiyama, Eiji
Currie, Thayne
Mayama, Satoshi
Takami, Michihiro
Thalmann, Christian
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Abe, Lyu
Brandner, Wolfgang
Brandt, Timothy D.
Carson, Joseph C.
Egner, Sebastian
Feldt, Markus
Goto, Miwa
Grady, Carol A.
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko S.
Henning, Thomas
Hodapp, Klaus W.
Ishii, Miki
Iye, Masanori
Janson, Markus
Kandori, Ryo
Knapp, Gillian R.
Kuzuhara, Masayuki
Kwon, Jungmi
Matsuo, Taro
McElwain, Michael W.
Miyama, Shoken
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishimura, Tetsuo
Pyo, Tae-Soo
Serabyn, Eugene
Suenaga, Takuya
Suto, Hiroshi
Suzuki, Ryuji
Takahashi, Yasuhiro H.
Takato, Naruhisa
Terada, Hiroshi
Turner, Edwin L.
Watanabe, Makoto
Yamada, Toru
Takami, Hideki
Usuda, Tomonori
TI Near-infrared imaging polarimetry of LkCa 15: A possible warped inner
disk
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE circumstellar matter; protoplanetary disks; stars: individual (LkCa 15);
stars: pre-main-sequence
ID PROTOPLANETARY DISK; TW HYDRAE; PLANET; SYSTEM; GAP; EVOLUTION; IMAGES;
CAVITY; LIGHT; AU
AB We present high-contrast H-band polarized intensity images of the transitional disk around the young solar-like star LkCa 15. By utilizing Subaru/HiCIAO for polarimetric differential imaging, the angular resolution and the inner working angle reach 0.'' 07 and r = 0.'' 1, respectively. We obtained a clearly resolved gap (width less than or similar to 27 au) at similar to 48 au from the central star. This gap is consistent with images reported in previous studies. We also confirmed the existence of a bright inner disk with a misaligned position angle of 13 degrees +/- 4 degrees with respect to that of the outer disk, i. e., the inner disk is possibly warped. The large gap and the warped inner disk both point to the existence of a multiple planetary system with a mass of less than or similar to 1 M-Jup.
C1 [Oh, Daehyeon; Suenaga, Takuya] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Oh, Daehyeon; Tamura, Motohide; Akiyama, Eiji; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Suenaga, Takuya; Suto, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro H.; Terada, Hiroshi; Takami, Hideki; Usuda, Tomonori] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Hashimoto, Jun; Tamura, Motohide; Kusakabe, Nobuhiko; Suto, Hiroshi] Natl Inst Nat Sci, Astrobiol Ctr, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Tamura, Motohide; Kwon, Jungmi; Takahashi, Yasuhiro H.] Univ Tokyo, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
[Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA.
[Currie, Thayne; Kudo, Tomoyuki; Egner, Sebastian; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko S.; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa] Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA.
[Mayama, Satoshi] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan.
[Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
[Thalmann, Christian] Swiss Fed Inst Technol, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Abe, Lyu] Univ Nice Sophia Antipolis, Lab Lagrange, UMR 7293, Observ Cote Azur,CNRS, 28 Ave Valrose, F-06108 Nice 2, France.
[Brandner, Wolfgang; Henning, Thomas] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Brandt, Timothy D.; Feldt, Markus] Inst Adv Study, Dept Astrophys, Olden Lane, Princeton, NJ 08540 USA.
[Carson, Joseph C.] Coll Charleston, Dept Phys & Astron, 58 Coming St, Charleston, SC 29424 USA.
[Goto, Miwa] Univ Munich, Univ Sternwarte Munchen, Scheinerstr 1, D-81679 Munich, Germany.
[Grady, Carol A.; McElwain, Michael W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA.
[Grady, Carol A.] Eureka Sci, 2452 Delmer,Suite 100, Oakland, CA 96002 USA.
[Grady, Carol A.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Hodapp, Klaus W.] Univ Hawaii, Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA.
[Janson, Markus; Knapp, Gillian R.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan.
[Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan.
[Miyama, Shoken] Hiroshima Univ, 1-3-2 Kagamiyama, Hiroshima 7398511, Japan.
[Moro-Martin, Amaya] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Moro-Martin, Amaya] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA.
[Serabyn, Eugene; Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778568, Japan.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Oh, D (reprint author), Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.; Oh, D (reprint author), Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
EM daehyun.oh@nao.ac.jp
RI MIYAMA, Shoken/A-3598-2015;
OI Feldt, Markus/0000-0002-4188-5242
FU [15H02063]
FX We are grateful to an anonymous referee for providing many useful
comments leading to an improved version of this letter. We are grateful
for the assistance of the Subaru telescope. This work makes use of data
provided by SMOKA (Baba et al. 2002). MT is supported by Grant-in-Aid
for Scientific Research (No. 15H02063).
NR 31
TC 1
Z9 1
U1 2
U2 5
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD APR
PY 2016
VL 68
IS 2
AR L3
DI 10.1093/pasj/psv133
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ9ZK
UT WOS:000374571900001
ER
PT J
AU Nayagam, V
Dietrich, DL
Williams, FA
AF Nayagam, Vedha
Dietrich, Daniel L.
Williams, Forman A.
TI Partial-Burning Regime for Quasi-Steady Droplet Combustion Supported by
Cool Flames
SO AIAA JOURNAL
LA English
DT Article
ID N-HEPTANE; MICROGRAVITY; EXTINCTION
AB A simplified model for droplet combustion in the partial-burning regime is applied to the cool-flame regime observed in droplet-burning experiments performed in the International Space Station with normal-alkanes fuels resulting in expressions for the quasi-steady droplet burning rate and for the flame standoff ratio. The simplified predictions are found to produce reasonable agreement with the experimentally measured values of burning-rate constants but not with their apparent dependencies on pressure or on the initial droplet diameter. Good agreement is found, however, with newly measured and numerically calculated flame standoff ratios in this droplet combustion supported by cool flames.
C1 [Nayagam, Vedha] Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA.
[Dietrich, Daniel L.] NASA, John H Glenn Res Ctr, Dept Mech & Aerosp Engn, Cleveland, OH 44135 USA.
[Williams, Forman A.] Univ Calif San Diego, Dept Mech & Aerosp Engn, La Jolla, CA 92093 USA.
RP Nayagam, V (reprint author), Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA.
FU NASA Space Life and Physical Sciences Research and Applications Program;
International Space Station Program
FX This work was supported by the NASA Space Life and Physical Sciences
Research and Applications Program, and the International Space Station
Program. J. Mark Hickman served as the project manager.
NR 13
TC 3
Z9 3
U1 5
U2 6
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD APR
PY 2016
VL 54
IS 4
BP 1235
EP 1239
DI 10.2514/1.J054437
PG 5
WC Engineering, Aerospace
SC Engineering
GA DK4HH
UT WOS:000374877600008
ER
PT J
AU Acero, F
Ackermann, M
Ajello, M
Albert, A
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bellazzini, R
Bissaldi, E
Bloom, ED
Bonino, R
Bottacini, E
Brandt, TJ
Bregeon, J
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caragiulo, M
Caraveo, PA
Casandjian, JM
Cavazzuti, E
Cecchi, C
Charles, E
Chekhtman, A
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cuoco, A
Cutini, S
D'Ammando, F
de Angelis, A
de Palma, F
Desiante, R
Digel, SW
Di Venere, L
Drell, PS
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Franckowiak, A
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Guiriec, S
Hadasch, D
Harding, AK
Hayashi, K
Hays, E
Hewitt, JW
Hill, AB
Horan, D
Hou, X
Jogler, T
Johannesson, G
Kamae, T
Kuss, M
Landriu, D
Larsson, S
Latronico, L
Li, J
Li, L
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Maldera, S
Malyshev, D
Manfreda, A
Martin, P
Mayer, M
Mazziotta, MN
McEnery, JE
Michelson, PF
Mirabal, N
Mizuno, T
Monzani, ME
Morselli, A
Nuss, E
Ohsugi, T
Omodei, N
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Pesce-Rollins, M
Piron, F
Pivato, G
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Remy, Q
Renault, N
Sanchez-Conde, M
Schaal, M
Schulz, A
Sgro, C
Siskind, EJ
Spada, F
Spandre, G
Spinelli, P
Strong, AW
Suson, DJ
Tajima, H
Takahashi, H
Thayer, JB
Thompson, DJ
Tibaldo, L
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Vianello, G
Werner, M
Wood, KS
Wood, M
Zaharijas, G
Zimmer, S
AF Acero, F.
Ackermann, M.
Ajello, M.
Albert, A.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bellazzini, R.
Bissaldi, E.
Bloom, E. D.
Bonino, R.
Bottacini, E.
Brandt, T. J.
Bregeon, J.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Caraveo, P. A.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cuoco, A.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Desiante, R.
Digel, S. W.
Di Venere, L.
Drell, P. S.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Franckowiak, A.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Guiriec, S.
Hadasch, D.
Harding, A. K.
Hayashi, K.
Hays, E.
Hewitt, J. W.
Hill, A. B.
Horan, D.
Hou, X.
Jogler, T.
Johannesson, G.
Kamae, T.
Kuss, M.
Landriu, D.
Larsson, S.
Latronico, L.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Maldera, S.
Malyshev, D.
Manfreda, A.
Martin, P.
Mayer, M.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mirabal, N.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Nuss, E.
Ohsugi, T.
Omodei, N.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Remy, Q.
Renault, N.
Sanchez-Conde, M.
Schaal, M.
Schulz, A.
Sgro, C.
Siskind, E. J.
Spada, F.
Spandre, G.
Spinelli, P.
Strong, A. W.
Suson, D. J.
Tajima, H.
Takahashi, H.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Vianello, G.
Werner, M.
Wood, K. S.
Wood, M.
Zaharijas, G.
Zimmer, S.
TI DEVELOPMENT OF THE MODEL OF GALACTIC INTERSTELLAR EMISSION FOR STANDARD
POINT-SOURCE ANALYSIS OF FERMI LARGE AREA TELESCOPE DATA
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE gamma rays: diffuse background; gamma rays: general; gamma rays: ISM
ID GAMMA-RAY EMISSION; COSMIC-RAY; MOLECULAR CLOUDS; MILKY-WAY;
RADIAL-DISTRIBUTION; EGRET OBSERVATIONS; HELIUM SPECTRA; COLUMN DENSITY;
X-RAY; PARTICLE-PRODUCTION
AB Most of the celestial. rays detected by the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope originate from the interstellar medium when energetic cosmic rays interact with interstellar nucleons and photons. Conventional point-source and extended-source studies rely on the modeling of this diffuse emission for accurate characterization. Here, we describe the development of the Galactic Interstellar Emission Model (GIEM), which is the standard adopted by the LAT Collaboration and is publicly available. This model is based on a linear combination of maps for interstellar gas column density in Galactocentric annuli and for the inverse-Compton emission produced in the Galaxy. In the GIEM, we also include large-scale structures like Loop. I and the Fermi bubbles. The measured gas emissivity spectra confirm that the cosmic-ray proton density decreases with Galactocentric distance beyond 5 kpc from the Galactic Center. The measurements also suggest a softening of the proton spectrum with Galactocentric distance. We observe that the Fermi bubbles have boundaries with a shape similar to a catenary at latitudes below 20 degrees and we observe an enhanced emission toward their base extending in the north and south Galactic directions and located within similar to 4 degrees of the Galactic Center.
C1 [Acero, F.; Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Landriu, D.; Remy, Q.; Renault, N.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France.
[Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Albert, A.; Baldini, L.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Michelson, P. F.; Monzani, M. E.; Omodei, N.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Reimer, A.; Reimer, O.; Tajima, H.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Albert, A.; Baldini, L.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Jogler, T.; Michelson, P. F.; Monzani, M. E.; Omodei, N.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Reimer, A.; Reimer, O.; Tajima, H.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.; Bellazzini, R.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Chiaro, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bissaldi, E.; Caragiulo, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bonino, R.; Cuoco, A.; Desiante, R.; Latronico, L.; Maldera, S.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bonino, R.; Cuoco, A.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[Brandt, T. J.; Buson, S.; Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hays, E.; McEnery, J. E.; Mirabal, N.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34059 Montpellier, France.
[Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Buson, S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Buson, S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Buson, S.] CRESST, Greenbelt, MD 20771 USA.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] ASI Sci Data Ctr, I-00133 Rome, Italy.
[Cecchi, C.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Roma, Italy.
[Conrad, J.; Sanchez-Conde, M.; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.; Larsson, S.; Li, L.; Sanchez-Conde, M.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Funk, S.; Malyshev, D.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Hayashi, K.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
[Hewitt, J. W.] Univ N Florida, Dept Phys, 1 UNF Dr, Jacksonville, FL 32224 USA.
[Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Hou, X.] Chinese Acad Sci, Yunnan Observ, Kunming 650216, Peoples R China.
[Hou, X.] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650216, Peoples R China.
[Johannesson, G.] Univ Iceland, Inst Sci, Dunhaga 3, IS-107 Reykjavik, Iceland.
[Kamae, T.] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
[Larsson, S.; Li, L.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Li, J.; Torres, D. F.] Inst Space Sci IEEC CSIC, Campus UAB, E-08193 Barcelona, Spain.
[Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Martin, P.] CNRS, IRAP, F-31028 Toulouse 4, France.
[McEnery, J. E.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Razzaque, S.] Univ Johannesburg, Dept Phys, POB 524, ZA-2006 Auckland Pk, South Africa.
[Schaal, M.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Schaal, M.] Naval Res Lab, Washington, DC 20375 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Zaharijas, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Zaharijas, G.] Univ Trieste, I-34127 Trieste, Italy.
[Zaharijas, G.] Univ Nova Gor, Lab Astroparticle Phys, Vipavska 13, SI-5000 Nova Gorica, Slovenia.
RP Casandjian, JM; Grenier, IA (reprint author), Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France.
EM casandjian@cea.fr; isabelle.grenier@cea.fr
RI Bissaldi, Elisabetta/K-7911-2016; Reimer, Olaf/A-3117-2013; Orlando,
E/R-5594-2016; Funk, Stefan/B-7629-2015; Bonino, Raffaella/S-2367-2016;
Torres, Diego/O-9422-2016; Di Venere, Leonardo/C-7619-2017;
OI Bissaldi, Elisabetta/0000-0001-9935-8106; Reimer,
Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Torres,
Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X;
Sgro', Carmelo/0000-0001-5676-6214; Zaharijas,
Gabrijela/0000-0001-8484-7791; Pesce-Rollins,
Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094;
Mazziotta, Mario Nicola/0000-0001-9325-4672; Ajello,
Marco/0000-0002-6584-1703
FU National Aeronautics and Space Administration in the United States;
Department of Energy in the United States; Commissariat a l'Energie
Atomique in France; Centre National de la Recherche
Scientifique/Institut National de Physique Nucleaire et de Physique des
Particules in France; Agenzia Spaziale Italiana in Italy; Istituto
Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture,
Sports, Science and Technology (MEXT) in Japan; High Energy Accelerator
Research Organization (KEK) in Japan; Japan Aerospace Exploration Agency
(JAXA) in Japan; KA Wallenberg Foundation in Sweden; Swedish Research
Council in Sweden; Swedish National Space Board in Sweden; Istituto
Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in
France
FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the KA Wallenberg Foundation, the Swedish
Research Council, and the Swedish National Space Board in Sweden.;
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France.
NR 137
TC 24
Z9 24
U1 7
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD APR
PY 2016
VL 223
IS 2
AR 26
DI 10.3847/0067-0049/223/2/26
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DL0EI
UT WOS:000375304600008
ER
PT J
AU Bhat, PN
Meegan, CA
von Kienlin, A
Paciesas, WS
Briggs, MS
Burgess, JM
Burns, E
Chaplin, V
Cleveland, WH
Collazzi, AC
Connaughton, V
Diekmann, AM
Fitzpatrick, G
Gibby, MH
Giles, MM
Goldstein, AM
Greiner, J
Jenke, PA
Kippen, RM
Kouveliotou, C
Mailyan, B
McBreen, S
Pelassa, V
Preece, RD
Roberts, OJ
Sparke, LS
Stanbro, M
Veres, P
Wilson-Hodge, CA
Xiong, SL
Younes, G
Yu, HF
Zhang, BB
AF Bhat, P. Narayana
Meegan, Charles A.
von Kienlin, Andreas
Paciesas, William S.
Briggs, Michael S.
Burgess, J. Michael
Burns, Eric
Chaplin, Vandiver
Cleveland, William H.
Collazzi, Andrew C.
Connaughton, Valerie
Diekmann, Anne M.
Fitzpatrick, Gerard
Gibby, Melissa H.
Giles, Misty M.
Goldstein, Adam M.
Greiner, Jochen
Jenke, Peter A.
Kippen, R. Marc
Kouveliotou, Chryssa
Mailyan, Bagrat
McBreen, Sheila
Pelassa, Veronique
Preece, Robert D.
Roberts, Oliver J.
Sparke, Linda S.
Stanbro, Matthew
Veres, Peter
Wilson-Hodge, Colleen A.
Xiong, Shaolin
Younes, George
Yu, Hoi-Fung
Zhang, Binbin
TI THE THIRD FERMI GBM GAMMA-RAY BURST CATALOG: THE FIRST SIX YEARS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; gamma-ray burst: general
ID MONITOR; FLASHES; TRIGGER; ORIGIN; BATSE; GRBS
AB Since its launch in 2008, the Fermi Gamma-ray Burst Monitor (GBM) has triggered and located on average approximately two.-ray bursts (GRBs) every three days. Here, we present the third of a series of catalogs of GRBs detected by GBM, extending the second catalog by two more years through the middle of 2014 July. The resulting list includes 1405 triggers identified as GRBs. The intention of the GBM GRB catalog is to provide information to the community on the most important observables of the GBM-detected GRBs. For each GRB, the location and main characteristics of the prompt emission, the duration, peak flux, and fluence are derived. The latter two quantities are calculated for the 50-300 keV energy band where the maximum energy release of GRBs in the instrument reference system is observed, and also for a broader energy band from 10 to 1000 keV, exploiting the full energy range of GBM's low-energy [NaI[Tl)] detectors. Using statistical methods to assess clustering, we find that the hardness and duration of GRBs are better fit by a two-component model with short-hard and long-soft bursts than by a model with three components. Furthermore, information is provided on the settings and modifications of the triggering criteria and exceptional operational conditions during years five and six in the mission. This third catalog is an official product of the Fermi GBM science team, and the data files containing the complete results are available from the High-Energy Astrophysics Science Archive Research Center.
C1 [Bhat, P. Narayana; Meegan, Charles A.; Briggs, Michael S.; Burns, Eric; Chaplin, Vandiver; Fitzpatrick, Gerard; Jenke, Peter A.; Mailyan, Bagrat; Pelassa, Veronique; Stanbro, Matthew; Veres, Peter; Zhang, Binbin] Univ Alabama, CSPAR, 320 Sparkman Dr, Huntsville, AL 35805 USA.
[Bhat, P. Narayana; Briggs, Michael S.; Connaughton, Valerie; Jenke, Peter A.; Preece, Robert D.] Univ Alabama, Dept Space Sci, 320 Sparkman Dr, Huntsville, AL 35899 USA.
[von Kienlin, Andreas; Greiner, Jochen; Yu, Hoi-Fung] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Paciesas, William S.; Cleveland, William H.; Connaughton, Valerie] Univ Space Res Assoc, 320 Sparkman Dr, Huntsville, AL 35805 USA.
[Burgess, J. Michael] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Burgess, J. Michael] AlbaNova Univ Ctr, KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden.
[Chaplin, Vandiver] Vanderbilt Univ, Inst Imaging Sci, 1161 21st Ave South,Med Ctr North,AA 1105, Nashville, TN 37232 USA.
[Collazzi, Andrew C.] SciTec Inc, 100 Wall St, Princeton, NJ 08540 USA.
[Diekmann, Anne M.; Gibby, Melissa H.; Giles, Misty M.] Jacobs Technol Inc, Huntsville, AL USA.
[Fitzpatrick, Gerard; McBreen, Sheila; Roberts, Oliver J.] Univ Coll Dublin, Sch Phys, Stillorgan Rd, Dublin 4, Ireland.
[Goldstein, Adam M.; Wilson-Hodge, Colleen A.] NASA, George C Marshall Space Flight Ctr, Astrophys Off ZP12, Huntsville, AL 35812 USA.
[Greiner, Jochen; Yu, Hoi-Fung] Tech Univ Munich, Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany.
[Kippen, R. Marc] Los Alamos Natl Lab, MS B244,POB 1663, Los Alamos, NM 87545 USA.
[Kouveliotou, Chryssa; Younes, George] George Washington Univ, Dept Phys, 725 21st St NW, Washington, DC 20052 USA.
[Pelassa, Veronique] Fred Lawrence Whipple Observ, 670 Mt Hopkins Rd, Amado, AZ 85645 USA.
[Sparke, Linda S.] NASA, HQ, Sci Mission Directorate, Astrophys, 300 E St SW, Washington, DC 20546 USA.
[Xiong, Shaolin] Inst High Energy Phys, Key Lab Particle Astrophys, 19B Yuquan Rd, Beijing 100049, Peoples R China.
[Zhang, Binbin] CSIC, IAA, POB 03004, E-18080 Granada, Spain.
RP Bhat, PN (reprint author), Univ Alabama, CSPAR, 320 Sparkman Dr, Huntsville, AL 35805 USA.; Bhat, PN (reprint author), Univ Alabama, Dept Space Sci, 320 Sparkman Dr, Huntsville, AL 35899 USA.
RI Roberts, Oliver/N-6284-2016;
OI Roberts, Oliver/0000-0002-7150-9061; von Kienlin,
Andreas/0000-0002-0221-5916; Burgess, James/0000-0003-3345-9515;
McBreen, Sheila/0000-0002-1477-618X
FU Bundesministerium fur Bildung und Forschung (BMBF) via the Deutsches
Zentrum fur Luft und Raumfahrt (DLR) [50 QV 0301]; Bundesministeriums
fur Wirtschaft und Technologie (BMWi) through DLR [50 OG 1101]; Science
Foundation Ireland [12/IP/1288]; DFG cluster of excellence "Origin and
Structure of the universe"; NASA Postdoctoral Program through Oak Ridge
Associated Universities; NASA [NNM11AA01A]
FX Support for the German contribution to G.B.M. was provided by the
Bundesministerium fur Bildung und Forschung (BMBF) via the Deutsches
Zentrum fur Luft und Raumfahrt (DLR) under contract number 50 QV 0301.
A.v.K. was supported by the Bundesministeriums fur Wirtschaft und
Technologie (BMWi) through DLR grant 50 OG 1101. S.M. B. and O.J.R.
acknowledge support from Science Foundation Ireland under grant No.
12/IP/1288. H.F.Y. acknowledges support by the DFG cluster of excellence
"Origin and Structure of the universe." A.G. is funded by the NASA
Postdoctoral Program through Oak Ridge Associated Universities. The UAH
co-authors gratefully acknowledge NASA funding from co-operative
agreement NNM11AA01A. C.K. and C.A.W.H. gratefully acknowledge NASA
funding through the Fermi GBM project.
NR 44
TC 4
Z9 4
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD APR
PY 2016
VL 223
IS 2
AR 28
DI 10.3847/0067-0049/223/2/28
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DL0EI
UT WOS:000375304600010
ER
PT J
AU van der Wel, A
Noeske, K
Bezanson, R
Pacifici, C
Gallazzi, A
Franx, M
Munoz-Mateos, JC
Bell, EF
Brammer, G
Charlot, S
Chauke, P
Labbe, I
Maseda, MV
Muzzin, A
Rix, HW
Sobral, D
van de Sande, J
van Dokkum, PG
Wild, V
Wolf, C
AF van der Wel, A.
Noeske, K.
Bezanson, R.
Pacifici, C.
Gallazzi, A.
Franx, M.
Munoz-Mateos, J. C.
Bell, E. F.
Brammer, G.
Charlot, S.
Chauke, P.
Labbe, I.
Maseda, M. V.
Muzzin, A.
Rix, H. -W.
Sobral, D.
van de Sande, J.
van Dokkum, P. G.
Wild, V.
Wolf, C.
TI THE VLT LEGA-C SPECTROSCOPIC SURVEY: THE PHYSICS OF GALAXIES AT A
LOOKBACK TIME OF 7 Gyr
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: evolution; galaxies: fundamental parameters; galaxies:
general; galaxies: stellar content; surveys
ID STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; TULLY-FISHER RELATION;
SIMILAR-TO 2; ACTIVE GALACTIC NUCLEI; STELLAR MASS DENSITY;
SPACE-TELESCOPE OBSERVATIONS; DISTANT FIELD GALAXIES; HIGH-REDSHIFT
GALAXIES; GREATER-THAN 1
AB The Large Early Galaxy Census (LEGA-C-16) is a Public Spectroscopic Survey of similar to 3200 K-band selected galaxies at redshifts z. =. 0.6 - 1.0 with stellar masses M-* > 10(10) M-circle dot, conducted with VIMOS on ESO's Very Large Telescope. The survey is embedded in the COSMOS field (R.A. = 10h00; decl. = +2 deg). The 20 hr long integrations produce high-signal-to-noise ratio continuum spectra that reveal ages, metallicities and velocity dispersions of the stellar populations. LEGA-C's unique combination of sample size and depth will enable us for the first time to map the stellar content at large lookback time, across galaxies of different types and star formation activity. Observations started in 2014 December and are planned to be completed by mid 2018, with early data releases of the spectra and value-added products. In this paper we present the science case, the observing strategy, an overview of the data reduction process and data products, and a first look at the relationship between galaxy structure and spectral properties, as it existed 7 Gyr ago.
C1 [van der Wel, A.; Noeske, K.; Chauke, P.; Rix, H. -W.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Bezanson, R.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Pacifici, C.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
[Gallazzi, A.] INAF Osservatorio Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy.
[Franx, M.; Labbe, I.; Maseda, M. V.; Sobral, D.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 AA Leiden, Netherlands.
[Munoz-Mateos, J. C.] European So Observ, Alonso de Crdova 3107,Casilla 19001, Santiago, Chile.
[Bell, E. F.] Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA.
[Brammer, G.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Charlot, S.] UPMC CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Muzzin, A.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Sobral, D.] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England.
[van de Sande, J.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[van Dokkum, P. G.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Wild, V.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Wolf, C.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
RP van der Wel, A (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM vdwel@mpia.de
RI Sobral, David/C-7919-2014;
OI Sobral, David/0000-0001-8823-4845; Gallazzi, Anna/0000-0002-9656-1800;
Bell, Eric/0000-0002-5564-9873; Brammer, Gabriel/0000-0003-2680-005X
FU Deutsche Forschungsemeinschaft [GZ: WE 4755/4-1]; NASA - Space Telescope
Science Institute [HF-51318]; NASA [NAS 5-26555]; NWO Spinoza grant;
European Research Council
FX We thank the referee for a thorough reading of the manuscript and
constructive comments. A.W. and K.N. acknowledge support from the
Deutsche Forschungsemeinschaft (GZ: WE 4755/4-1). R.B. gratefully
acknowledges support by NASA through Hubble Fellowship grants #HF-51318
awarded by the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., for
NASA, under contract NAS 5-26555. C.P. acknowledges support by an
appointment to the NASA Postdoctoral Program at the Goddard Space Flight
Center, administered by USRA through a contract with NASA. We gratfeully
acknowledge the NWO Spinoza grant. V.W. acknowledges support from the
European Research Council Starting Grant (SEDMorph; P.I. V. Wild).
NR 110
TC 2
Z9 2
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD APR
PY 2016
VL 223
IS 2
AR 29
DI 10.3847/0067-0049/223/2/29
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DL0EI
UT WOS:000375304600011
ER
PT J
AU Hitlin, D
Kim, JH
Trevor, J
Hennessy, J
Hoenk, M
Jewell, A
Farrell, R
McClish, M
AF Hitlin, David
Kim, Jae Hong
Trevor, Jason
Hennessy, John
Hoenk, Michael
Jewell, April
Farrell, Richard
McClish, Mickel
TI An APD for the Detection of the Fast Scintillation Component of BaF2
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE Optical sensors
AB Barium fluoride crystals are the baseline choice for the calorimeter of the Mu2e experiment at Fermilab. By utilizing the fast 220 nm scintillation component (0.9 ns decay time) and discriminating against the larger slow component at 300 nm (650 ns decay time), it is possible to build a radiation hard calorimeter with good energy and time resolution and high rate capability. This requires a solid state photosensor with high quantum efficiency at 220 nm, discrimination against the 300 nm component, and fast rise and decay times. Progress on the development of such a sensor will be discussed.
C1 [Hitlin, David; Kim, Jae Hong; Trevor, Jason] CALTECH, Lauritsen Lab, Pasadena, CA 91125 USA.
[Hennessy, John; Hoenk, Michael; Jewell, April] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Farrell, Richard; McClish, Mickel] RMD Inc, Watertown, MA 02472 USA.
RP Hitlin, D (reprint author), CALTECH, Lauritsen Lab, Pasadena, CA 91125 USA.
EM hitlin@caltech.edu
FU Caltech; RMD Inc. under SBIR [DE-SC0011316]; NASA; Department of Energy;
Jet Propulsion Laboratory
FX This work was supported by a collaborative effort of Caltech, the Jet
Propulsion Laboratory, and RMD Inc., under SBIR grant DE-SC0011316, and
by NASA and the Department of Energy.
NR 12
TC 0
Z9 0
U1 2
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD APR
PY 2016
VL 63
IS 2
BP 513
EP 515
DI 10.1109/TNS.2016.2527651
PN 1
PG 3
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA DK6JF
UT WOS:000375028700016
ER
PT J
AU Tang, A
Kim, Y
Chang, MCF
AF Tang, Adrian
Kim, Yangyho
Chang, Mau-Chung Frank
TI Logic-I/O Threshold Comparing gamma-Dosimeter in Radiation Insensitive
Deep-Sub-Micron CMOS
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE Advanced CMOS; CMOS dosimeter; deep-sub-micron technology
AB This paper discusses challenges of implementing embedded dosimeters into larger CMOS systems-on-chip (SoCs) in deep-scaled CMOS technologies (with gate lengths smaller than 90 nm) where the high level of intrinsic radiation hardness and limited availability of floating gate structures prohibit realizing a highly sensitive radfet-type dosimeter. We therefore propose a novel Logic-I/O Threshold Comparison Dosimeter, which offers compatibility with advanced CMOS technology nodes and co-integration with other circuitry. The proposed dosimeter estimates dose level by directly comparing threshold voltages between I/O and logic devices. Furthermore, through carefully sizing the logic and I/O devices and designing the vital comparator circuitry, we can also achieve required temperature independence for deep-space applications. A prototype is then fabricated in 65-nm CMOS, and measured up to 75 Mrad(Si) of total ionized dose at a Cobalt 60 (gamma) facility.
C1 [Tang, Adrian] CALTECH, Jet Prop Lab, Instruments Div, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Tang, Adrian; Kim, Yangyho; Chang, Mau-Chung Frank] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA.
RP Tang, A (reprint author), CALTECH, Jet Prop Lab, Instruments Div, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Kim, Y; Chang, MCF (reprint author), Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA.
EM ajtang@jpl.nasa.gov; rod.m.kim@gmail.com; mfchang@ee.ucla.edu
NR 9
TC 1
Z9 1
U1 3
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD APR
PY 2016
VL 63
IS 2
BP 1247
EP 1250
DI 10.1109/TNS.2016.2528219
PN 3
PG 4
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA DK6LQ
UT WOS:000375035800020
ER
PT J
AU Abraham, E
Havelund, K
AF Abraham, Erika
Havelund, Klaus
TI Some recent advances in automated analysis
SO INTERNATIONAL JOURNAL ON SOFTWARE TOOLS FOR TECHNOLOGY TRANSFER
LA English
DT Article
DE Analysis; Parallel algorithms; Satisfiability modulo theories; Runtime
verification; Probabilistic systems
ID EFFICIENT SMT-SOLVER; MODEL CHECKING; PROGRAMS; SATISFIABILITY; TIME
AB Due to the increasing complexity of software systems, there is a growing need for automated and scalable software synthesis and analysis. In the last decade, active research in the formal methods community brought interesting results and valuable tools. However, there are still challenges to face and hard problems that need to be solved. We briefly outline some recent trends, and review some of the latest achievements, introducing six papers selected from the 20th International Conference on Tools and Algorithms for the Construction and Analysis of Systems (TACAS 2014).
C1 [Abraham, Erika] Rhein Westfal TH Aachen, Aachen, Germany.
[Havelund, Klaus] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Havelund, K (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM Klaus.Havelund@jpl.nasa.gov
RI Abraham, Erika/G-5259-2012
OI Abraham, Erika/0000-0002-5647-6134
NR 82
TC 0
Z9 0
U1 2
U2 2
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1433-2779
EI 1433-2787
J9 INT J SOFTW TOOLS TE
JI Int. J. Softw. Tools Technol. Transf.
PD APR
PY 2016
VL 18
IS 2
BP 121
EP 128
DI 10.1007/s10009-015-0403-0
PG 8
WC Computer Science, Software Engineering
SC Computer Science
GA DK5QQ
UT WOS:000374975200001
ER
PT J
AU von Essen, C
Giannakopoulou, D
AF von Essen, Christian
Giannakopoulou, Dimitra
TI Probabilistic verification and synthesis of the next generation airborne
collision avoidance system
SO INTERNATIONAL JOURNAL ON SOFTWARE TOOLS FOR TECHNOLOGY TRANSFER
LA English
DT Article
DE Markov decision processes; Probabilistic verification; Probabilistic
synthesis; Aircraft collision avoidance
ID CONFLICT-RESOLUTION
AB The next generation airborne collision avoidance system, ACAS X, departs from the traditional deterministic model on which the current system, TCAS, is based. To increase robustness, ACAS X relies on probabilistic models to represent the various sources of uncertainty. The work reported in this paper identifies verification challenges for ACAS X, and studies the applicability of probabilistic verification and synthesis techniques in addressing these challenges. Due to shortcomings of off-the-shelf probabilistic analysis tools, we developed a new framework, named VERICA (Verification for Collision Avoidance). VERICA is a combined probabilistic synthesis and verification framework that is custom designed for ACAS X and systems with similar characteristics. VERICA supports Java as a modeling language, is memory efficient, employs parallelization, and provides an interactive simulator that displays aircraft encounters and the corresponding ACAS X behavior. We describe the application of our framework to ACAS X, together with the results and recommendations that our analysis produced.
C1 [von Essen, Christian] Verimag, Grenoble, France.
[Giannakopoulou, Dimitra] NASA Ames Res Ctr, Moffett Field, CA USA.
RP Giannakopoulou, D (reprint author), NASA Ames Res Ctr, Moffett Field, CA USA.
EM vonessen.christian@gmail.com; dimitra.giannakopoulou@nasa.gov
NR 20
TC 1
Z9 1
U1 0
U2 2
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1433-2779
EI 1433-2787
J9 INT J SOFTW TOOLS TE
JI Int. J. Softw. Tools Technol. Transf.
PD APR
PY 2016
VL 18
IS 2
BP 227
EP 243
DI 10.1007/s10009-015-0388-8
PG 17
WC Computer Science, Software Engineering
SC Computer Science
GA DK5QQ
UT WOS:000374975200007
ER
PT J
AU Bandyopadhyay, S
Chung, SJ
Hadaegh, FY
AF Bandyopadhyay, Saptarshi
Chung, Soon-Jo
Hadaegh, Fred Y.
TI Nonlinear Attitude Control of Spacecraft with a Large Captured Object
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation, and Control Conference
CY JAN 05-09, 2015
CL Kissimmee, FL
SP AIAA
ID RODRIGUES PARAMETERS; CONTRACTION ANALYSIS; LAGRANGIAN SYSTEMS; RIGID
SPACECRAFT; ADAPTIVE-CONTROL; TRACKING CONTROL; SYNCHRONIZATION;
STABILIZATION; MANEUVERS; MOTION
AB This paper presents an attitude control strategy and a new nonlinear tracking controller for a spacecraft carrying a large object, such as an asteroid or a boulder. If the captured object is larger or comparable in size to the spacecraft and has significant modeling uncertainties, conventional nonlinear control laws that use exact feedforward cancellation are not suitable because they exhibit a large resultant disturbance torque. The proposed nonlinear tracking control law guarantees global exponential convergence of tracking errors with finite-gainLp stability in the presence of modeling uncertainties and disturbances, and it reduces the resultant disturbance torque. Furthermore, this control law permits the use of any attitude representation, and its integral control formulation eliminates any constant disturbance. Under small uncertainties, the best strategy for stabilizing the combined system is to track a fuel-optimal reference trajectory using this nonlinear control law because it consumes the least amount of fuel. In the presence of large uncertainties, the most effective strategy is to track the derivative plus proportional-derivative-based reference trajectory because it reduces the resultant disturbance torque. The effectiveness of the proposed attitude control methods is demonstrated by using results of numerical simulation based on an Asteroid Redirect Mission concept.
C1 [Bandyopadhyay, Saptarshi] Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.
[Chung, Soon-Jo] Univ Illinois, Dept Aerosp Engn, Coordinated Sci Lab, Urbana, IL 61801 USA.
[Hadaegh, Fred Y.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Bandyopadhyay, S (reprint author), Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.; Chung, SJ (reprint author), Univ Illinois, Dept Aerosp Engn, Coordinated Sci Lab, Urbana, IL 61801 USA.; Hadaegh, FY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM bandyop2@illinois.edu; sjchung@illinois.edu; fred.y.hadaegh@jpl.nasa.gov
NR 38
TC 1
Z9 1
U1 2
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD APR
PY 2016
VL 39
IS 4
BP 754
EP 769
DI 10.2514/1.G001341
PG 16
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA DK4BH
UT WOS:000374861000002
ER
PT J
AU Olson, CG
Russell, RP
Carpenter, JR
AF Olson, Corwin G.
Russell, Ryan P.
Carpenter, J. Russell
TI Small-Body Optical Navigation Using the Additive Divided Difference
Sigma Point Filter
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID MODIFIED RODRIGUES PARAMETERS; SMALL BODIES; ALGORITHM
C1 [Olson, Corwin G.] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, 1 Univ Stn, Austin, TX 78712 USA.
[Russell, Ryan P.] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, 1 Univ Stn,C0600, Austin, TX 78712 USA.
[Carpenter, J. Russell] NASA, Goddard Space Flight Ctr, Nav & Miss Design Branch, Greenbelt, MD 20771 USA.
RP Olson, CG (reprint author), Univ Texas Austin, Dept Aerosp Engn & Engn Mech, 1 Univ Stn, Austin, TX 78712 USA.
FU NASA's Chief Technology Office through a NASA Space Technology Research
Fellowship grant [NNX12AM60H]
FX The work described in this Note was funded by NASA's Chief Technology
Office through a NASA Space Technology Research Fellowship grant
(NNX12AM60H).
NR 29
TC 0
Z9 0
U1 1
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD APR
PY 2016
VL 39
IS 4
BP 920
EP 926
DI 10.2514/1.G001160
PG 7
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA DK4BH
UT WOS:000374861000015
ER
PT J
AU Shen, JW
Singleton, JD
Piatak, DJ
Bauchau, OA
Masarati, P
AF Shen, Jinwei
Singleton, Jeffrey D.
Piatak, David J.
Bauchau, Olivier A.
Masarati, Pierangelo
TI Multibody Dynamics Simulation and Experimental Investigation of a
Model-Scale Tiltrotor
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
ID WHIRL-FLUTTER STABILITY; SYSTEMS
AB The objective of this investigation is to illustrate the steps involved in developing a multibody dynamics analytical model to simulate the aeroelastic stability and blade loading of a soft-inplane tiltrotor wind tunnel model and to correlate those simulations with experimental data. Development of soft-inplane tiltrotor technology is beneficial for providing viable lightweight hub design options for future heavy lift transport rotorcraft application. Experimental verification of such advanced configurations using either subscale models in wind tunnels or full-scale flight testing is becoming prohibitively expensive. Advanced modeling and simulation of complex tiltrotor hub configurations using multibody dynamics analyses offers an alternative to such expensive experimental verifications. Comprehensive rotorcraft-oriented multibody analyses enable the modeling and simulation of rotor hub systems to a level of detail that allows the complex kinematics and nonlinear effects associated with rotor hub control systems and drive train free play to be considered. The influence of these and other nonlinear effects on the aeromechanical behavior of a tiltrotor model is examined in this study.
C1 [Shen, Jinwei] Natl Inst Aerosp, Hampton, VA USA.
[Singleton, Jeffrey D.] US Army Res & Technol, Basic Res, Crystal City, VA USA.
[Piatak, David J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Bauchau, Olivier A.] Univ Maryland, College Pk, MD 20742 USA.
[Masarati, Pierangelo] Politecn Milan, Dipartimento Ingn Aerosp, I-20133 Milan, Italy.
[Shen, Jinwei] Univ Alabama, Tuscaloosa, AL USA.
RP Shen, JW (reprint author), Univ Alabama, Tuscaloosa, AL USA.
EM jinwei.shen@eng.ua.edu
RI Masarati, Pierangelo/I-3898-2012
OI Masarati, Pierangelo/0000-0002-9347-7654
NR 24
TC 0
Z9 0
U1 5
U2 9
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
EI 2161-6027
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD APR
PY 2016
VL 61
IS 2
AR 022010
DI 10.4050/JAHS.61.022010
PG 11
WC Engineering, Aerospace
SC Engineering
GA DK3UI
UT WOS:000374842500010
ER
PT J
AU Hartwig, J
Vera, J
AF Hartwig, Jason
Vera, Jesus
TI Numerical Modeling of the Transient Chilldown of a Cryogenic Propellant
Transfer Line
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
ID HEAT-TRANSFER; FLOW
AB Before cryogenic fuel depots can be fully realized, efficient methods with which to chill down the spacecraft transfer line and receiver tank are required. This paper presents numerical modeling of the chilldown of a liquid hydrogen tank-to-tank propellant transfer line using the Generalized Fluid System Simulation Program. To compare with data from recently concluded turbulent liquid hydrogen chilldown experiments, seven different cases were run across a range of inlet liquid temperatures and mass flow rates. Both trickle and pulse chilldown methods were simulated. The Generalized Fluid System Simulation Program model qualitatively matches external skin-mounted temperature readings, but large differences are shown between measured and predicted internal stream temperatures. Discrepancies are attributed to the simplified model correlation used to compute two-phase flow, boiling heat transfer. Flow visualization from testing shows that the initial bottoming out of skin-mounted sensors corresponds to annular flow but that considerable time is required for the stream sensor to achieve steady state as the system moves through annular, churn, and bubbly flows. The Generalized Fluid System Simulation Program model does adequately well in tracking trends in the data, but further work is needed to refine the two-phase flow modeling to better match observed test data.
C1 [Hartwig, Jason] NASA, John H Glenn Res Ctr, Propellants & Prop Branch, 21000 Brookpark Rd,MS 301-3, Brookpark, OH 44142 USA.
[Vera, Jesus] NASA, John H Glenn Res Ctr, Fluids Syst Branch, 21000 Brookpark Rd,MS 301-3, Brookpark, OH 44142 USA.
RP Hartwig, J (reprint author), NASA, John H Glenn Res Ctr, Propellants & Prop Branch, 21000 Brookpark Rd,MS 301-3, Brookpark, OH 44142 USA.
FU Cryogenic Propellant Storage and Transfer Project under the Space
Technology Mission Directorate at NASA
FX This work was funded by the Cryogenic Propellant Storage and Transfer
Project under the Space Technology Mission Directorate at NASA.
NR 21
TC 1
Z9 1
U1 3
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0887-8722
EI 1533-6808
J9 J THERMOPHYS HEAT TR
JI J. Thermophys. Heat Transf.
PD APR
PY 2016
VL 30
IS 2
BP 403
EP 409
DI 10.2514/1.T4725
PG 7
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA DK4CA
UT WOS:000374863100016
ER
PT J
AU Patel, VK
Seyed-Yagoobi, J
Robinson, F
Didion, JR
AF Patel, Viral K.
Seyed-Yagoobi, Jamal
Robinson, Franklin
Didion, Jeffrey R.
TI Effect of Gravity on Electrohydrodynamic Conduction Driven Liquid Film
Flow Boiling
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
ID MICROGRAVITY; TERRESTRIAL; FIELD
AB Liquid film flow boiling is used in many terrestrial thermal management applications as a heat transport mechanism. However, it suffers in microgravity applications such as spacecraft thermal management because the gravitational body force is not present to facilitate liquid film flow and bubble removal from the heater surface. One way of overcoming these constraints is to use an electrical field to move a liquid film in the absence as well as in the presence of gravity. In this experimental study, electrohydrodynamic conduction pumping is used to rewet the heater surface during liquid film flow boiling. The experiments are performed both terrestrially and onboard a variable-gravity parabolic flight. Terrestrial steady-state results show a maximum superheat reduction of 6 degrees C and a 62% increase in critical heat flux when the electrohydrodynamic pump is moderately activated. The parabolic flight transient results indicate that, although there was an adverse effect of electrohydrodynamic on heater surface temperature at heat flux less than 3.0 W/cm(2) (due to delayed onset of nucleate boiling), heater surface temperatures were actually lowered at higher heat flux due to activation of the electrohydrodynamic conduction pump. The microgravity results onboard the parabolic flights also pave the way for full-scale orbital testing of electrohydrodynamic-driven liquid film flow boiling onboard the International Space Station.
C1 [Patel, Viral K.] Worcester Polytech Inst, Multi Scale Heat Transfer Lab, Dept Mech Engn, Worcester, MA 01609 USA.
[Seyed-Yagoobi, Jamal] Worcester Polytech Inst, Dept Mech Engn, Worcester, MA 01609 USA.
[Robinson, Franklin] NASA, Goddard Space Flight Ctr, Thermal Technol Dev Lab, Greenbelt, MD 20771 USA.
[Didion, Jeffrey R.] NASA, Goddard Space Flight Ctr, Nanotechol Facil, Greenbelt, MD 20771 USA.
RP Patel, VK (reprint author), Worcester Polytech Inst, Multi Scale Heat Transfer Lab, Dept Mech Engn, Worcester, MA 01609 USA.; Patel, VK (reprint author), Oak Ridge Natl Lab, Bldg Equipment Res Grp, Energy & Transportat Sci Div, Oak Ridge, TN 37831 USA.
FU NASA Headquarters Micro-Gravity Fluid Physics Program
FX This project was financially supported by the NASA Headquarters
Micro-Gravity Fluid Physics Program.
NR 19
TC 0
Z9 0
U1 1
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0887-8722
EI 1533-6808
J9 J THERMOPHYS HEAT TR
JI J. Thermophys. Heat Transf.
PD APR
PY 2016
VL 30
IS 2
BP 429
EP 437
DI 10.2514/1.T4696
PG 9
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA DK4CA
UT WOS:000374863100019
ER
PT J
AU West, TK
Brune, AJ
Hosder, S
Johnston, CO
AF West, Thomas K.
Brune, Andrew J.
Hosder, Serhat
Johnston, Christopher O.
TI Uncertainty Analysis of Radiative Heating Predictions for Titan Entry
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
ID LUNAR-RETURN CONDITIONS; SHOCK-LAYER RADIATION; POLYNOMIAL CHAOS;
SENSITIVITY-ANALYSIS; ATMOSPHERIC ENTRY; REENTRY FLOWS; QUANTIFICATION;
SIMULATIONS; METHODOLOGY; MODEL
AB The objective of this study was to investigate the uncertainty in shock layer radiative heating predictions on the surface of a hypersonic inflatable aerodynamic decelerator during Titan entry at peak radiative heating conditions. Computational fluid dynamics simulations of planetary entry flows and radiative heating predictions possess a significant amount of uncertainty due to the complexity of the flow physics and the difficulty in obtaining accurate experimental results of molecular-level phenomena. Sources of uncertainty considered include flowfield chemical rate models, molecular band emission, and the excitation/deexcitation rates of molecules modeled with a non-Boltzmann approach. Because of the computational cost of the numerical models, uncertainty quantification was performed with a surrogate modeling approach based on a sparse approximation of the point-collocation nonintrusive polynomial chaos expansion. Accurate uncertainty results were obtained with only 500 evaluations of the computational model. Results showed that epistemic uncertainty intervals of surface radiative heating predictions were as wide as 150 W/cm(2) during Titan entry, indicating the significant effect of uncertainty. A global nonlinear sensitivity analysis showed that the top uncertainty source contributing to the uncertainty in radiative heating was the flowfield chemistry modeling throughout the shock layer.
C1 [West, Thomas K.; Brune, Andrew J.] Missouri Univ Sci & Technol, Dept Aerosp & Mech Engn, Rolla, MO 65409 USA.
[Hosder, Serhat] Missouri Univ Sci & Technol, Dept Aerosp & Mech Engn, Aerosp Engn, Rolla, MO 65409 USA.
[Johnston, Christopher O.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
RP West, TK (reprint author), Missouri Univ Sci & Technol, Dept Aerosp & Mech Engn, Rolla, MO 65409 USA.
NR 56
TC 1
Z9 1
U1 1
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0887-8722
EI 1533-6808
J9 J THERMOPHYS HEAT TR
JI J. Thermophys. Heat Transf.
PD APR
PY 2016
VL 30
IS 2
BP 438
EP 451
DI 10.2514/1.T4620
PG 14
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA DK4CA
UT WOS:000374863100020
ER
PT J
AU Omidy, AD
Panerai, F
Lachaud, JR
Mansour, NN
Martin, A
AF Omidy, Ali D.
Panerai, Francesco
Lachaud, Jean R.
Mansour, Nagi N.
Martin, Alexandre
TI Effects of Water Phase Change on the Material Response of Low-Density
Carbon-Phenolic Ablators
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
ID CHARRING ABLATIVE MATERIALS; PYROLYSIS-GAS; REAXFF; DFTB
C1 [Omidy, Ali D.; Panerai, Francesco; Martin, Alexandre] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Lachaud, Jean R.] Univ Calif Santa Cruz, Silicon Valley Initiat, Moffett Field, CA 94043 USA.
[Mansour, Nagi N.] NASA, Ames Res Ctr, Modeling & Simulat, TN Div, Moffett Field, CA 94043 USA.
RP Omidy, AD; Panerai, F; Martin, A (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.; Lachaud, JR (reprint author), Univ Calif Santa Cruz, Silicon Valley Initiat, Moffett Field, CA 94043 USA.; Mansour, NN (reprint author), NASA, Ames Res Ctr, Modeling & Simulat, TN Div, Moffett Field, CA 94043 USA.
EM ali.omidy2@uky.edu; francesco.panerai@uky.edu; jlachaud@ucsc.edu;
nagi.n.mansour@nasa.gov; alexandre.martin@uky.edu
OI Martin, Alexandre/0000-0003-2216-2468; Lachaud, Jean/0000-0001-7397-1025
FU NASA Kentucky EPSCoR award [NNX13AN04A]; NASA Kentucky Space Grant
[NNX10AL96H]; NASA [NNX14AC93A, NNX14AI97G]
FX Financial support for this work was provided in part by NASA Kentucky
EPSCoR award NNX13AN04A, NASA Kentucky Space Grant award NNX10AL96H,
NASA award NNX14AC93A, and NASA award NNX14AI97G. Part of this work was
also performed under the Entry System Modeling Project (M. J. Wright,
project manager) of the NASA Game Changing Development Program. A. D.
Omidy is thankful to D. B. Hash and the summer program at NASA Ames
Research Center, as well as M. Mahzari, A. J. Amar, and T. R. White for
the numerous insightful discussions. Finally, the authors are grateful
to S. C. C. Bailey, K. A. Tagavi, M. J. Wright, A. Vanaerschot, B. A.
Biegel, and D. B. Hash for carefully reviewing the manuscript.
NR 38
TC 1
Z9 1
U1 10
U2 14
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0887-8722
EI 1533-6808
J9 J THERMOPHYS HEAT TR
JI J. Thermophys. Heat Transf.
PD APR
PY 2016
VL 30
IS 2
BP 472
EP 477
DI 10.2514/1.T4814
PG 6
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA DK4CA
UT WOS:000374863100024
ER
PT J
AU Bi, J
Myneni, R
Lyapustin, A
Wang, YJ
Park, T
Chi, C
Yan, K
Knyazikhin, Y
AF Bi, Jian
Myneni, Ranga
Lyapustin, Alexei
Wang, Yujie
Park, Taejin
Chi, Chen
Yan, Kai
Knyazikhin, Yuri
TI Amazon Forests' Response to Droughts: A Perspective from the MAIAC
Product
SO REMOTE SENSING
LA English
DT Article
DE Amazon forests; photosynthesis; remote sensing; MODIS; MAIAC; drought
ID MODIS CLOUD MASK; ATMOSPHERIC CORRECTION; VEGETATION INDEXES; CARBON
DYNAMICS; SENSITIVITY; IMPACT; DEGRADATION; SEASONALITY; PATTERNS; MODEL
AB Amazon forests experienced two severe droughts at the beginning of the 21st century: one in 2005 and the other in 2010. How Amazon forests responded to these droughts is critical for the future of the Earth's climate system. It is only possible to assess Amazon forests' response to the droughts in large areal extent through satellite remote sensing. Here, we used the Multi-Angle Implementation of Atmospheric Correction (MAIAC) Moderate Resolution Imaging Spectroradiometer (MODIS) vegetation index (VI) data to assess Amazon forests' response to droughts, and compared the results with those from the standard (Collection 5 and Collection 6) MODIS VI data. Overall, the MAIAC data reveal more realistic Amazon forests inter-annual greenness dynamics than the standard MODIS data. Our results from the MAIAC data suggest that: (1) the droughts decreased the greenness (i.e., photosynthetic activity) of Amazon forests; (2) the Amazon wet season precipitation reduction induced by El Nino events could also lead to reduced photosynthetic activity of Amazon forests; and (3) in the subsequent year after the water stresses, the greenness of Amazon forests recovered from the preceding decreases. However, as previous research shows droughts cause Amazon forests to reduce investment in tissue maintenance and defense, it is not clear whether the photosynthesis of Amazon forests will continue to recover after future water stresses, because of the accumulated damages caused by the droughts.
C1 [Bi, Jian; Myneni, Ranga; Park, Taejin; Chi, Chen; Yan, Kai; Knyazikhin, Yuri] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Lyapustin, Alexei; Wang, Yujie] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bi, Jian] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
RP Bi, J (reprint author), Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.; Bi, J (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
EM bijian.bj@gmail.com; ranga.myneni@gmail.com;
alexei.i.lyapustin@nasa.gov; yujie.wang-1@nasa.gov;
taejin1392@gmail.com; chenchi@bu.edu; kaiyan@bu.edu; jknjazi@bu.edu
RI Myneni, Ranga/F-5129-2012
FU NASA Earth Science Division; Aligned Research Program of UC Santa Cruz
FX This research was funded by NASA Earth Science Division. J.B. also
acknowledges support from the Aligned Research Program of UC Santa Cruz.
NR 42
TC 2
Z9 2
U1 6
U2 14
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD APR
PY 2016
VL 8
IS 4
AR 356
DI 10.3390/rs8040356
PG 12
WC Remote Sensing
SC Remote Sensing
GA DK8DD
UT WOS:000375156500089
ER
PT J
AU Gong, WY
Thiele, A
Hinz, S
Meyer, FJ
Hooper, A
Agram, PS
AF Gong, Wenyu
Thiele, Antje
Hinz, Stefan
Meyer, Franz J.
Hooper, Andrew
Agram, Piyush S.
TI Comparison of Small Baseline Interferometric SAR Processors for
Estimating Ground Deformation
SO REMOTE SENSING
LA English
DT Article
DE interferometry; synthetic aperture radar; time series; deformation
monitoring
ID APERTURE RADAR INTERFEROMETRY; LOS-ANGELES BASIN; TIME-SERIES; INSAR;
ALGORITHM; SCATTERERS; ALASKA; INTERFEROGRAMS; COHERENCE; VOLCANO
AB The small Baseline Synthetic Aperture Radar (SAR) Interferometry (SBI) technique has been widely and successfully applied in various ground deformation monitoring applications. Over the last decade, a variety of SBI algorithms have been developed based on the same fundamental concepts. Recently developed SBI toolboxes provide an open environment for researchers to apply different SBI methods for various purposes. However, there has been no thorough discussion that compares the particular characteristics of different SBI methods and their corresponding performance in ground deformation reconstruction. Thus, two SBI toolboxes that implement a total of four SBI algorithms were selected for comparison. This study discusses and summarizes the main differences, pros and cons of these four SBI implementations, which could help users to choose a suitable SBI method for their specific application. The study focuses on exploring the suitability of each SBI module under various data set conditions, including small/large number of interferograms, the presence or absence of larger time gaps, urban/vegetation ground coverage, and temporally regular/irregular ground displacement with multiple spatial scales. Within this paper we discuss the corresponding theoretical background of each SBI method. We present a performance analysis of these SBI modules based on two real data sets characterized by different environmental and surface deformation conditions. The study shows that all four SBI processors are capable of generating similar ground deformation results when the data set has sufficient temporal sampling and a stable ground backscatter mechanism like urban area. Strengths and limitations of different SBI processors were analyzed based on data set configuration and environmental conditions and are summarized in this paper to guide future users of SBI techniques.
C1 [Gong, Wenyu; Meyer, Franz J.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
[Thiele, Antje; Hinz, Stefan] Karlsruhe Inst Technol, Inst Photogrammetry & Remote Sensing, D-76131 Karlsruhe, Germany.
[Hooper, Andrew] Univ Leeds, COMET, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Agram, Piyush S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gong, WY (reprint author), Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
EM gwenyu@alaska.edu; antje.thiele@kit.edu; stefan.hinz@kit.edu;
fjmeyer@alaska.edu; A.Hooper@leeds.ac.uk; Piyush.Agram@jpl.nasa.gov
OI , Wenyu/0000-0001-6806-8974; Hooper, Andrew/0000-0003-4244-6652
FU Alaska Satellite Facility
FX We would like to thank all the anonymous reviewers for their insightful
comments on the paper. ERS data is provided by European Space Agency
(ESA) through WInSAR and Envisat data is provided by ESA. The GPS data
in LA test site is obtained through the service provided by UNAVCO
(http://facility.unavco.org/data/dai2/app/dai2.html). The land cover
data is provided by National Land Cover Database 2006
(http://www.mrlc.gov/nlcd2006.php). We thank Jeff Freymueller from
University of Alaska Fairbanks for sharing the GPS position field data
at Okmok Volcano test site. We thank Robin Falge from Karlsruhe
Institute of Technology for providing the important data processing
support. The StaMPS/MTI package is available from
http://homepages.see.leeds.ac.uk/similar to earahoo/stamps/ and GIAnT
package is available from http://earthdef.caltech.edu/. This research
has also obtained the great support from Alaska Satellite Facility.
COMET is the NERC Centre for the Observation and Modelling of
Earthquakes, Volcanoes and Tectonics.
NR 65
TC 1
Z9 1
U1 1
U2 6
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD APR
PY 2016
VL 8
IS 4
AR 330
DI 10.3390/rs8040330
PG 26
WC Remote Sensing
SC Remote Sensing
GA DK8DD
UT WOS:000375156500063
ER
PT J
AU Lagomasino, D
Fatoyinbo, T
Lee, S
Feliciano, E
Trettin, C
Simard, M
AF Lagomasino, David
Fatoyinbo, Temilola
Lee, SeungKuk
Feliciano, Emanuelle
Trettin, Carl
Simard, Marc
TI A Comparison of Mangrove Canopy Height Using Multiple Independent
Measurements from Land, Air, and Space
SO REMOTE SENSING
LA English
DT Article
DE canopy height; DSM; biomass; Africa; H100; blue carbon; TDX; VHR; MRV
ID POLARIMETRIC SAR INTERFEROMETRY; CARBON-DIOXIDE EMISSIONS; RAIN-FOREST
LANDSCAPE; POL-INSAR; TANDEM-X; ZAMBEZI DELTA; TREE HEIGHT; SATELLITE;
LIDAR; BIOMASS
AB Canopy height is one of the strongest predictors of biomass and carbon in forested ecosystems. Additionally, mangrove ecosystems represent one of the most concentrated carbon reservoirs that are rapidly degrading as a result of deforestation, development, and hydrologic manipulation. Therefore, the accuracy of Canopy Height Models (CHM) over mangrove forest can provide crucial information for monitoring and verification protocols. We compared four CHMs derived from independent remotely sensed imagery and identified potential errors and bias between measurement types. CHMs were derived from three spaceborne datasets; Very-High Resolution (VHR) stereophotogrammetry, TerraSAR-X add-on for Digital Elevation Measurement, and Shuttle Radar Topography Mission (TanDEM-X), and lidar data which was acquired from an airborne platform. Each dataset exhibited different error characteristics that were related to spatial resolution, sensitivities of the sensors, and reference frames. Canopies over 10 m were accurately predicted by all CHMs while the distributions of canopy height were best predicted by the VHR CHM. Depending on the guidelines and strategies needed for monitoring and verification activities, coarse resolution CHMs could be used to track canopy height at regional and global scales with finer resolution imagery used to validate and monitor critical areas undergoing rapid changes.
C1 [Lagomasino, David] Univ Space Res Assoc, GESTAR, 7178 Columbia Gateway Dr, Columbia, MD 21046 USA.
[Lagomasino, David; Fatoyinbo, Temilola; Lee, SeungKuk; Feliciano, Emanuelle] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Trettin, Carl] USDA, Forest Serv, Cordesville, SC 29434 USA.
[Simard, Marc] Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lagomasino, D (reprint author), Univ Space Res Assoc, GESTAR, 7178 Columbia Gateway Dr, Columbia, MD 21046 USA.; Lagomasino, D (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM david.lagomasino@nasa.gov; lola.fatoyinbo@nasa.gov;
seungkuk.lee@nasa.gov; emanuelle.a.feliciano@nasa.gov;
ctrettin@fs.fed.us; marc.simard@jpl.nasa.gov
RI Fatoyinbo, Temilola/G-6104-2012; Lagomasino, David/P-8413-2015;
OI Fatoyinbo, Temilola/0000-0002-1130-6748; Lagomasino,
David/0000-0003-4008-5363; Trettin, Carl/0000-0003-0279-7191
FU NASA Carbon Monitoring Systems Program; USAID
FX This work was supported in part by the NASA Carbon Monitoring Systems
Program. The acquisition of the airborne lidar and MSS data were made
possible by funds from USAID support to the US Forest Service
International Programs Office under the USAID Mozambique Global Climate
Change Sustainable Landscape Program in support of the inventory of
carbon stocks in the Zambezi Delta. Commercial high-resolution imagery
from DigitalGlobe were obtained from NASA's Commercial Archive Data
website (cad4nasa.gsfc.nasa.gov) under the National
Geospatial-Intelligence Agency's NextView license agreement. We would
like to thank Jaime Nickeson for help in acquiring the commercial
imagery from NGA. Part of this work was performed at the Jet Propulsion
Laboratory, California Institute of Technology.
NR 54
TC 1
Z9 1
U1 11
U2 19
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD APR
PY 2016
VL 8
IS 4
AR 327
DI 10.3390/rs8040327
PG 18
WC Remote Sensing
SC Remote Sensing
GA DK8DD
UT WOS:000375156500060
ER
PT J
AU Bertincourt, B
Lagache, G
Martin, PG
Schulz, B
Conversi, L
Dassas, K
Maurin, L
Abergel, A
Beelen, A
Bernard, JP
Crill, BP
Dole, H
Eales, S
Gudmundsson, JE
Lellouch, E
Moreno, R
Perdereau, O
AF Bertincourt, B.
Lagache, G.
Martin, P. G.
Schulz, B.
Conversi, L.
Dassas, K.
Maurin, L.
Abergel, A.
Beelen, A.
Bernard, J-P.
Crill, B. P.
Dole, H.
Eales, S.
Gudmundsson, J. E.
Lellouch, E.
Moreno, R.
Perdereau, O.
TI Comparison of absolute gain photometric calibration between Planck/HFI
and Herschel/SPIRE at 545 and 857 GHz
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE methods: data analysis
ID IRAS
AB We compare the absolute gain photometric calibration of the Planck/HFI and Herschel/SPIRE instruments on diffuse emission. The absolute calibration of HFI and SPIRE each relies on planet flux measurements and comparison with theoretical far-infrared emission models of planetary atmospheres. We measure the photometric cross calibration between the instruments at two overlapping bands, 545GHz/500 mu m and 857 GHz/350 mu m. The SPIRE maps used have been processed in the Herschel Interactive Processing Environment (Version 12) and the HFI data are from the 2015 Public Data Release 2. For our study we used 15 large fields observed with SPIRE, which cover a total of about 120 deg(2). We have selected these fields carefully to provide high signal-to-noise ratio, avoid residual systematics in the SPIRE maps, and span a wide range of surface brightness. The HFI maps are bandpass-corrected to match the emission observed by the SPIRE bandpasses. The SPIRE maps are convolved to match the HFI beam and put on a common pixel grid. We measure the cross-calibration relative gain between the instruments using two methods in each field, pixel-to-pixel correlation and angular power spectrum measurements. The SPIRE/HFI relative gains are 1.047 (+/- 0.0069) and 1.003 (+/- 0.0080) at 545 and 857 GHz, respectively, indicating very good agreement between the instruments. These relative gains deviate from unity by much less than the uncertainty of the absolute extended emission calibration, which is about 6.4% and 9.5% for HFI and SPIRE, respectively, but the deviations are comparable to the values 1.4% and 5.5% for HFI and SPIRE if the uncertainty from models of the common calibrator can be discounted. Of the 5.5% uncertainty for SPIRE, 4% arises from the uncertainty of the effective beam solid angle, which impacts the adopted SPIRE point source to extended source unit conversion factor, highlighting that as a focus for refinement.
C1 [Bertincourt, B.; Lagache, G.; Dassas, K.; Abergel, A.; Beelen, A.; Dole, H.] Univ Paris 11, CNRS, UMR 8617, IAS, Bat 121, F-91405 Orsay, France.
[Lagache, G.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada.
[Schulz, B.] IPAC, NASA Herschel Sci Ctr, 770 South Wilson Ave, Pasadena, CA 91125 USA.
[Conversi, L.] ESA, European Space Astron Ctr ESAC, Madrid 28691, Spain.
[Maurin, L.] Univ Paris 07, APC, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France.
[Bernard, J-P.] CNRS, IRAP, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France.
[Bernard, J-P.] Univ Toulouse, UPS, OMP, IRAP, F-31028 Toulouse 4, France.
[Crill, B. P.] CALTECH, Dept Phys, 4800 Oak Grove Dr, Pasadena, CA USA.
[Crill, B. P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA.
[Eales, S.] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales.
[Gudmundsson, J. E.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Lellouch, E.; Moreno, R.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, 5 Pl J Janssen, F-92195 Meudon, France.
[Perdereau, O.] Univ Paris 11, Lab Accelerateur Lineaire, CNRS, IN2P3, F-91898 Orsay, France.
RP Lagache, G (reprint author), Univ Paris 11, CNRS, UMR 8617, IAS, Bat 121, F-91405 Orsay, France.; Lagache, G (reprint author), Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
EM guilaine.lagache@lam.fr
FU CNES; ESA; CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF
(Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain);
MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland);
CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space
(Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES
(Portugal); ERC; PRACE (EU)
FX We thank Jean-Loup Puget for insightful discussions. B.B. is
particularly thankful to Marc-Antoine Miville-Deschenes for providing us
pre-release access to the Spider SPIRE data. B.B. acknowledges the
support of a CNES post-doctoral research grant. We thank the referee,
Bernard Lazareff, for helpful comments that have led to improvements in
the manuscript. The Planck Collaboration acknowledges the support of:
ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy);
NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES
(Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA
(Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI
(Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of
the Planck Collaboration and a list of its members, indicating which
technical or scientific activities they have been involved in, can be
found at http://www.cosmos.esa.int/web/planck/planck-collaboration.
NR 28
TC 4
Z9 4
U1 1
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2016
VL 588
AR A107
DI 10.1051/0004-6361/201527313
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0SQ
UT WOS:000373207800119
ER
PT J
AU Gatuzz, E
Garcia, JA
Kallman, TR
Mendoza, C
AF Gatuzz, Efrain
Garcia, Javier A.
Kallman, Timothy R.
Mendoza, Claudio
TI Oxygen, neon, and iron X-ray absorption in the local interstellar medium
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: general; ISM: atoms; ISM: abundances; ISM: structure; X-rays: ISM
ID HOT INTERGALACTIC MEDIUM; XMM-NEWTON OBSERVATION; K ABSORPTION;
PHYSICAL-PROPERTIES; ATOMIC OXYGEN; SCULPTOR WALL; SPECTROSCOPY;
BINARIES; SPECTRUM; EDGE
AB Aims. We present a detailed study of X-ray absorption in the local interstellar medium by analyzing the X-ray spectra of 24 galactic sources obtained with the Chandra High Energy Transmission Grating Spectrometer and the XMM-Newton Reflection Grating Spectrometer.
Methods. By modeling the continuum with a simple broken power-law and by implementing the new ISMabs X-ray absorption model, we have estimated the total H, O, Ne, and Fe column densities towards the observed sources.
Results. We have determined the absorbing material distribution as a function of source distance and galactic latitude-longitude.
Conclusions. Direct estimates of the fractions of neutrally, singly, and doubly ionized species of O, Ne, and Fe reveal the dominance of the cold component, thus indicating an overall low degree of ionization. Our results are expected to be sensitive to the model used to describe the continuum in all sources.
C1 [Gatuzz, Efrain] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Gatuzz, Efrain] Cent Univ Venezuela, Fac Ciencias, Escuela Fis, POB 20632, Caracas 1020A, Venezuela.
[Gatuzz, Efrain; Mendoza, Claudio] Inst Venezolano Invest Cient, Ctr Fis, POB 20632, Caracas 1020A, Venezuela.
[Garcia, Javier A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Kallman, Timothy R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gatuzz, E (reprint author), Max Planck Inst Astrophys, D-85741 Garching, Germany.; Gatuzz, E (reprint author), Cent Univ Venezuela, Fac Ciencias, Escuela Fis, POB 20632, Caracas 1020A, Venezuela.; Gatuzz, E (reprint author), Inst Venezolano Invest Cient, Ctr Fis, POB 20632, Caracas 1020A, Venezuela.
EM egatuzz@mpa-garching.mpg.de
NR 43
TC 2
Z9 2
U1 1
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2016
VL 588
AR A111
DI 10.1051/0004-6361/201527752
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0SQ
UT WOS:000373207800123
ER
PT J
AU Goetz, C
Koenders, C
Richter, I
Altwegg, K
Burch, J
Carr, C
Cupido, E
Eriksson, A
Guttler, C
Henri, P
Mokashi, P
Nemeth, Z
Nilsson, H
Rubin, M
Sierks, H
Tsurutani, B
Vallat, C
Volwerk, M
Glassmeier, KH
AF Goetz, C.
Koenders, C.
Richter, I.
Altwegg, K.
Burch, J.
Carr, C.
Cupido, E.
Eriksson, A.
Guettler, C.
Henri, P.
Mokashi, P.
Nemeth, Z.
Nilsson, H.
Rubin, M.
Sierks, H.
Tsurutani, B.
Vallat, C.
Volwerk, M.
Glassmeier, K. -H.
TI First detection of a diamagnetic cavity at comet
67P/Churyumov-Gerasimenko
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE comets: individual: 67P/Churyumov-Gerasimenko; plasmas; magnetic fields;
methods: data analysis
ID SOLAR-WIND; ROSETTA; IONOPAUSE; PLASMA; HALLEY; MAGNETOMETER; STABILITY;
REGION; SYSTEM
AB Context. The Rosetta magnetometer RPC-MAG has been exploring the plasma environment of comet 67P/Churyumov-Gerasimenko since August 2014. The first months were dominated by low-frequency waves which evolved into more complex features. However, at the end of July 2015, close to perihelion, the magnetometer detected a region that did not contain any magnetic field at all.
Aims. These signatures match the appearance of a diamagnetic cavity as was observed at comet 1P/Halley in 1986. The cavity here is more extended than previously predicted by models and features unusual magnetic field configurations, which need to be explained.
Methods. The onboard magnetometer data were analyzed in detail and used to estimate the outgassing rate. A minimum variance analysis was used to determine boundary normals.
Results. Our analysis of the data acquired by the Rosetta Plasma Consortium instrumentation confirms the existence of a diamagnetic cavity. The size is larger than predicted by simulations, however. One possible explanation are instabilities that are propagating along the cavity boundary and possibly a low magnetic pressure in the solar wind. This conclusion is supported by a change in sign of the Sun-pointing component of the magnetic field. Evidence also indicates that the cavity boundary is moving with variable velocities ranging from 230 500m/s.
C1 [Goetz, C.; Koenders, C.; Richter, I.; Glassmeier, K. -H.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, Mendelssohnstr 3, D-38106 Braunschweig, Germany.
[Altwegg, K.; Rubin, M.] Univ Bern, Phys Inst, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Burch, J.; Mokashi, P.] Southwest Res Inst, PO Drawer 28510, San Antonio, TX 78228 USA.
[Carr, C.; Cupido, E.] Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, Exhibit Rd, London SW7 2AZ, England.
[Eriksson, A.] Swedish Inst Space Phys, Angstrom Lab, Lagerhyddsvagen 1, S-75105 Uppsala, Sweden.
[Guettler, C.; Sierks, H.] Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[Henri, P.] Univ Orleans, CNRS, Lab Phys & Chim Environm & Espace, UMR 7328, F-45100 Orleans, France.
[Nemeth, Z.] Wigner Res Ctr Phys, Konkoly Thege Miklos Ut 29-33, H-1121 Budapest, Hungary.
[Nilsson, H.] Swedish Inst Space Phys, POB 812, S-98128 Kiruna, Sweden.
[Tsurutani, B.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Vallat, C.] European Space Astron Ctr, Madrid 28691, Spain.
[Volwerk, M.] Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria.
RP Goetz, C (reprint author), Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, Mendelssohnstr 3, D-38106 Braunschweig, Germany.
EM c.goetz@tu-bs.de
RI Rubin, Martin/I-7777-2013
OI Rubin, Martin/0000-0001-6549-3318
FU German Ministerium fur Wirtschaft und Energie; Deutsches Zentrum fur
Luft- und Raumfahrt [50QP 1401]; federal state of Bern; Swiss National
Science Foundation; ESA PRODEX program; CNRS; CNES; Observatoire de
Paris and Universite Paul Sabatier; Toulouse and Imperial College
London; UK Science and Technology Facilities Council
FX The RPC-MAG and ROSINA data will be made available through the PSA
archive of ESA and the PDS archive of NASA. Rosetta is a European Space
Agency (ESA) mission with contributions from its member states and the
National Aeronautics and Space Administration (NASA). The work on
RPC-MAG was financially supported by the German Ministerium fur
Wirtschaft und Energie and the Deutsches Zentrum fur Luft- und Raumfahrt
under contract 50QP 1401. The work on ROSINA was funded by the federal
state of Bern, the Swiss National Science Foundation, and the ESA PRODEX
program. Portions of this research were performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA. We are indebted to the whole of the Rosetta Mission Team, SGS, and
RMOC for their outstanding efforts in making this mission possible. We
acknowledge the staff of CDDP and IC for the use of AMDA and the RPC
Quicklook database (provided by a collaboration between the Centre de
Donnees de la Physique des Plasmas, supported by CNRS, CNES,
Observatoire de Paris and Universite Paul Sabatier, Toulouse and
Imperial College London, supported by the UK Science and Technology
Facilities Council).
NR 23
TC 6
Z9 6
U1 6
U2 13
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2016
VL 588
AR A24
DI 10.1051/0004-6361/201527728
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0SQ
UT WOS:000373207800036
ER
PT J
AU Guidi, G
Tazzari, M
Testi, L
de Gregorio-Monsalvo, I
Chandler, CJ
Perez, L
Isella, A
Natta, A
Ortolani, S
Henning, T
Corder, S
Linz, H
Andrews, S
Wilner, D
Ricci, L
Carpenter, J
Sargent, A
Mundy, L
Storm, S
Calvet, N
Dullemond, C
Greaves, J
Lazio, J
Deller, A
Kwon, W
AF Guidi, G.
Tazzari, M.
Testi, L.
de Gregorio-Monsalvo, I.
Chandler, C. J.
Perez, L.
Isella, A.
Natta, A.
Ortolani, S.
Henning, Th.
Corder, S.
Linz, H.
Andrews, S.
Wilner, D.
Ricci, L.
Carpenter, J.
Sargent, A.
Mundy, L.
Storm, S.
Calvet, N.
Dullemond, C.
Greaves, J.
Lazio, J.
Deller, A.
Kwon, W.
TI Dust properties across the CO snowline in the HD 163296 disk from ALMA
and VLA observations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: pre-main sequence; protoplanetary disks; instrumentation:
interferometers; submillimeter: stars
ID T-TAURI STARS; PROTOPLANETARY DISKS; GRAIN-GROWTH; CIRCUMSTELLAR DISKS;
PLANET FORMATION; SOLAR NEBULA; HL TAU; MILLIMETER WAVELENGTHS;
ACCRETION DISKS; CQ TAURI
AB Context. To characterize the mechanisms of planet formation it is crucial to investigate the properties and evolution of protoplanetary disks around young stars, where the initial conditions for the growth of planets are set. The high spatial resolution of Atacama Large Millimeter/submillimeter Array (ALMA) and Karl G. Jansky Very Large Array (VLA) observations now allows the study of radial variations of dust properties in nearby resolved disks and the investigation of the early stages of grain growth in disk midplanes.
Aims. Our goal is to study grain growth in the well-studied disk of the young, intermediate-mass star HD 163296 where dust processing has already been observed and to look for evidence of growth by ice condensation across the CO snowline, which has already been identified in this disk with ALMA.
Methods. Under the hypothesis of optically thin emission, we compare images at different wavelengths from ALMA and VLA to measure the opacity spectral index across the disk and thus the maximum grain size. We also use a Bayesian tool based on a two-layer disk model to fit the observations and constrain the dust surface density.
Results. The measurements of the opacity spectral index indicate the presence of large grains and pebbles (>= 1 cm) in the inner regions of the disk (inside similar to 50 AU) and smaller grains, consistent with ISM sizes, in the outer disk (beyond 150 AU). Re-analyzing ALMA Band 7 science verification data, we find (radially) unresolved excess continuum emission centered near the location of the CO snowline at similar to 90 AU.
Conclusions. Our analysis suggests a grain size distribution consistent with an enhanced production of large grains at the CO snowline and consequent transport to the inner regions. Our results combined with the excess in infrared scattered light suggests there is a structure at 90 AU involving the whole vertical extent of the disk. This could be evidence of small scale processing of dust at the CO snowline.
C1 [Guidi, G.; Testi, L.; Natta, A.] Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy.
[Guidi, G.] Univ Florence, Dipartimento Fis & Astron, I-50121 Florence, Italy.
[Tazzari, M.; Testi, L.; de Gregorio-Monsalvo, I.] ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Tazzari, M.; Testi, L.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany.
[de Gregorio-Monsalvo, I.; Corder, S.] Joint ALMA Observ JAO, Alonso Cordova 3107 Vitacura, Santiago, Chile.
[Chandler, C. J.; Perez, L.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Isella, A.] Rice Univ, Dept Phys & Astron, 6100 Main St, Houston, TX 77005 USA.
[Natta, A.] Dublin Inst Adv Studies, Sch Cosm Phys, 31 Fitzwilliams Pl, Dublin 2, Ireland.
[Ortolani, S.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy.
[Ortolani, S.] Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy.
[Henning, Th.; Linz, H.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Andrews, S.; Wilner, D.; Ricci, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Carpenter, J.; Sargent, A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Mundy, L.; Storm, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Calvet, N.] Univ Michigan, Dept Astron, 830 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA.
[Dullemond, C.] Heidelberg Univ, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany.
[Greaves, J.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Lazio, J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Deller, A.] Netherlands Inst Radio Astron ASTRON, NL-7991 Dwingeloo, Netherlands.
[Kwon, W.] Korea Astron & Space Sci Inst, 776 Daedeok Daero, Daejeon 34055, South Korea.
RP Guidi, G (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy.
EM guidi@arcetri.astro.it
OI Dullemond, Cornelis/0000-0002-7078-5910
FU Italian Ministero dell'Istruzione, Universita e Ricerca [CUP
C52I13000140001]; National Aeronautics and Space Administration
FX This paper makes use of the following ALMA data:
ADS/JAO.ALMA#2011.0.000010.SV. ALMA is a partnership of ESO
(representing its member states), NSF (USA) and NINS (Japan), together
with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea),
in cooperation with the Republic of Chile. The Joint ALMA Observatory is
operated by ESO, AUI/NRAO and NAOJ. We are grateful to Antonio Garufi
for many discussions and for sharing his infrared polarization images.
We thank Sebastian Stammler for insightful discussions on the effect of
the CO snowline on dust and for showing us the results of his
simulations in advance of publication. We thank the anonymous referee
for the helpful comments. Part of this research was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. The
fits have been carried out on the computing facilities of the
Computational Center for Particle and Astrophysics (C2PAP) as part of
the approved project "Dust evolution in protoplanetary disks". M.T. and
L.T. are grateful for the experienced support by F. Beaujean (C2PAP).
This work was partly supported by the Italian Ministero dell'Istruzione,
Universita e Ricerca through the grant Progetti Premiali 2012 - iALMA
(CUP C52I13000140001).
NR 65
TC 8
Z9 8
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2016
VL 588
AR A112
DI 10.1051/0004-6361/201527516
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0SQ
UT WOS:000373207800124
ER
PT J
AU Kama, M
Bruderer, S
Carney, M
Hogerheijde, M
van Dishoeck, EF
Fedele, D
Baryshev, A
Boland, W
Gusten, R
Aikutalp, A
Choi, Y
Endo, A
Frieswijk, W
Karska, A
Klaassen, P
Koumpia, E
Kristensen, L
Leurini, S
Nagy, Z
Beaupuits, JPP
Risacher, C
van der Marel, N
van Kempen, TA
van Weeren, RJ
Wyrowski, F
Yildiz, UA
AF Kama, M.
Bruderer, S.
Carney, M.
Hogerheijde, M.
van Dishoeck, E. F.
Fedele, D.
Baryshev, A.
Boland, W.
Guesten, R.
Aikutalp, A.
Choi, Y.
Endo, A.
Frieswijk, W.
Karska, A.
Klaassen, P.
Koumpia, E.
Kristensen, L.
Leurini, S.
Nagy, Z.
Beaupuits, J. -P. Perez
Risacher, C.
van der Marel, N.
van Kempen, T. A.
van Weeren, R. J.
Wyrowski, F.
Yildiz, U. A.
TI Observations and modelling of CO and [CI] in protoplanetary disks First
detections of [CI] and constraints on the carbon abundance
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE surveys; protoplanetary disks; submillimeter: planetary systems
ID T-TAURI STARS; HERBIG AE/BE STARS; MAIN-SEQUENCE STARS; HD 100546; YOUNG
STARS; GAS-RICH; CIRCUMSTELLAR DISKS; VLBA DETERMINATION; TRANSITIONAL
DISK; ISO SPECTROSCOPY
AB Context. The gas-solid budget of carbon in protoplanetary disks is related to the composition of the cores and atmospheres of the planets forming in them. The principal gas-phase carbon carriers CO, C-0, and C+ can now be observed regularly in disks.
Aims. The gas-phase carbon abundance in disks has thus far not been well characterized observationally. We obtain new constraints on the [C]/[H] ratio in a large sample of disks, and compile an overview of the strength of [CI] and warm CO emission.
Methods. We carried out a survey of the CO 6-5 line and the [CI] 1-0 and 2-1 lines towards 37 disks with the APEX telescope, and supplemented it with [CII] data from the literature. The data are interpreted using a grid of models produced with the DALI disk code. We also investigate how well the gas-phase carbon abundance can be determined in light of parameter uncertainties.
Results. The CO6-5 line is detected in 13 out of 33 sources, [CI] 1-0 in 6 out of 12, and [CI] 2-1 in 1 out of 33. With separate deep integrations, the first unambiguous detections of the [CI] 1-0 line in disks are obtained, in TW Hya and HD 100546. Conclusions. Gas-phase carbon abundance reductions of a factor of 5-10 or more can be identified robustly based on CO and [CI] detections, assuming reasonable constraints on other parameters. The atomic carbon detection towards TW Hya confirms a factor of 100 reduction of [C]/[H](gas) in that disk, while the data are consistent with an ISM-like carbon abundance for HD 100546. In addition, BP Tau, T Cha, HD 139614, HD 141569, and HD 100453 are either carbon-depleted or gas-poor disks. The low [CI] 2-1 detection rates in the survey mostly reflect insufficient sensitivity for T Tauri disks. The Herbig Ae/Be disks with CO and [CII] upper limits below the models are debris-disk-like systems. An increase in sensitivity of roughly order of magnitude compared to our survey is required to obtain useful constraints on the gas-phase [C]/[H] ratio in most of the targeted systems.
C1 [Kama, M.; Carney, M.; Hogerheijde, M.; van Dishoeck, E. F.; Boland, W.; Frieswijk, W.; Klaassen, P.; Kristensen, L.; van der Marel, N.; van Kempen, T. A.; van Weeren, R. J.; Yildiz, U. A.] Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Bruderer, S.; Fedele, D.; Karska, A.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Baryshev, A.; Risacher, C.] SRON Netherlands Inst Space Res, NL-3584 Utrecht, Netherlands.
[Baryshev, A.; Aikutalp, A.; Choi, Y.; Koumpia, E.; Nagy, Z.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
[Boland, W.] NOVA, JH Oort Bldg,POB 9513, NL-2300 RA Leiden, Netherlands.
[Guesten, R.; Leurini, S.; Beaupuits, J. -P. Perez; Risacher, C.; Wyrowski, F.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Endo, A.] Delft Univ Technol, Kavli Inst Nanosci, Lorentzweg 1, NL-2628 CJ Delft, Netherlands.
[Frieswijk, W.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Karska, A.] Adam Mickiewicz Univ, Fac Phys, Astron Observ Inst, Sloneczna 36, PL-60286 Poznan, Poland.
[Klaassen, P.] Royal Observ, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Kristensen, L.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Nagy, Z.] Univ Toledo, Dept Phys & Astron, 2801 West Bancroft St, Toledo, OH 43606 USA.
[Yildiz, U. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Kama, M (reprint author), Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM mkama@strw.leidenuniv.nl
RI Fedele, Davide/L-8688-2013; Yildiz, Umut/C-5257-2011; Karska,
Agata/O-5311-2016; Kristensen, Lars E/F-4774-2011;
OI Fedele, Davide/0000-0001-6156-0034; Yildiz, Umut/0000-0001-6197-2864;
Karska, Agata/0000-0001-8913-925X; Kristensen, Lars
E/0000-0003-1159-3721; Kama, Mihkel/0000-0003-0065-7267; van Weeren,
Reinout/0000-0002-0587-1660
FU Royal Netherlands Academy of Arts and Sciences (KNAW); Netherlands
Research School for Astronomy (NOVA); European Union A-ERC grant [291141
CHEMPLAN]; Foundation for Polish Science (FNP); Polish National Science
Center [2013/11/N/ST9/00400]; NASA - Chandra X-ray Center [PF2-130104];
NASA [NAS8-03060]; Netherlands Organization for Scientific Research
(NWO) [600.063.310.10]
FX We thank the anonymous referee for constructive comments which helped to
improve the paper, Arnaud Belloche and the APEX staff for assistance
during the observations, and Matthijs van der Wiel for discussing his
SPIRE observations with us. This work is supported by a Royal
Netherlands Academy of Arts and Sciences (KNAW) professor prize, the
Netherlands Research School for Astronomy (NOVA), and by the European
Union A-ERC grant 291141 CHEMPLAN. A.K. acknowledges support from the
Foundation for Polish Science (FNP) and the Polish National Science
Center grant 2013/11/N/ST9/00400. R.J.W. is supported by NASA through
the Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra
X-ray Center, which is operated by the Smithsonian Astrophysical
Observatory for NASA under contract NAS8-03060. This publication is
based on data acquired with the Atacama Pathfinder Experiment (APEX).
APEX is a collaboration between the Max-Planck-Institut fur
Radioastronomie, the European Southern Observatory, and the Onsala Space
Observatory. CHAMP+ was constructed with support from the
Netherlands Organization for Scientific Research (NWO), grant
600.063.310.10.
NR 112
TC 10
Z9 10
U1 4
U2 5
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2016
VL 588
AR A108
DI 10.1051/0004-6361/201526791
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0SQ
UT WOS:000373207800120
ER
PT J
AU Pierbattista, M
Harding, AK
Gonthier, PL
Grenier, IA
AF Pierbattista, M.
Harding, A. K.
Gonthier, P. L.
Grenier, I. A.
TI Young and middle age pulsar light-curve morphology: Comparison of Fermi
observations with gamma-ray and radio emission geometries
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: neutron; pulsars: general; gamma rays: stars; radiation
mechanisms: non-thermal; methods: data analysis; methods: statistical
ID AREA TELESCOPE CATALOG; GAP MODEL; SLOT GAPS; POPULATION;
MAGNETOSPHERES; ACCELERATION
AB Thanks to the huge amount of gamma-ray pulsar photons collected by the Fermi Large Area Telescope since its launch in June 2008, it is now possible to constrain gamma-ray geometrical models by comparing simulated and observed light-curve morphological characteristics. We assumed vacuum-retarded dipole (VRD) pulsar magnetic field and tested simulated and observed morphological light-curve characteristics in the framework of two pole emission geometries, Polar Cap (PC) and Slot Gap (SG), and one pole emission geometries, traditional Outer Gap (OG) and One Pole Caustic (OPC). Radio core plus cone emission was assumed for the pulsars of the simulated sample. We compared simulated and observed recurrence of class shapes and peak multiplicity, peak separation, radio-lag distributions, and trends of peak separation and radio lag as a function of observable and non-observable pulsar parameters. We studied how pulsar morphological characteristics change in multi-dimensional observable and non-observable pulsar parameter space. The PC model gives the poorest description of the LAT pulsar light-curve morphology. The OPC best explains both the observed gamma-ray peak multiplicity and shape classes. The OPC and SG models describe the observed gamma-ray peak-separation distribution for low-and high-peak separations, respectively. This suggests that the OPC geometry best explains the single-peak structure but does not manage to describe the widely separated peaks predicted in the framework of the SG model as the emission from the two magnetic hemispheres. The OPC radio-lag distribution shows higher agreement with observations suggesting that assuming polar radio emission, the gamma-ray emission regions are likely to be located in the outer magnetosphere. Alternatively, the radio emission altitude could be higher that we assumed. We compared simulated non-observable parameters with the same parameters estimated for LAT pulsars in the framework of the same models. The larger agreement between simulated and LAT estimations in the framework of the OPC suggests that the OPC model best predicts the observed variety of profile shapes. The larger agreement obtained between observations and the OPC model predictions jointly with the need to explain the abundant 0.5 separated peaks with two-pole emission geometries, calls for thin OPC gaps to explain the single-peak geometry but highlights the need of two-pole caustic emission geometry to explain widely separated peaks.
C1 [Pierbattista, M.] Nicolaus Copernicus Astron Ctr, Rabianska 8, PL-87100 Torun, Poland.
[Pierbattista, M.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy.
[Harding, A. K.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gonthier, P. L.] Hope Coll, Dept Phys, Holland, MI 49423 USA.
[Grenier, I. A.] Univ Paris Diderot, Lab AIM, CEA Saclay, CEA,IRFU,CNRS,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Grenier, I. A.] Inst Univ France, F-75231 Paris 05, France.
RP Pierbattista, M (reprint author), Nicolaus Copernicus Astron Ctr, Rabianska 8, PL-87100 Torun, Poland.; Pierbattista, M (reprint author), Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy.
EM mpierba@gmail.com
FU Nicolaus Copernicus Astronomical Center [DEC-2011/02/A/ST9/00256];
National Science Foundation [AST-1009731, NNX09AQ71G]; Commonwealth
Government; Green Bank Telescope; National Science Foundation; Nancay
Radio Observatory; French Centre National de la Recherche Scientifique
(CNRS); Lowe telescope; Science and Technology Facilities Council of the
United Kingdom; Westerbork Synthesis Radio Telescope
FX The Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council and the Swedish National Space Board in Sweden.
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National etudes Spatiales in France. M. P.
acknowledges the Nicolaus Copernicus Astronomical Center, grant
DEC-2011/02/A/ST9/00256, for providing software and computer facilities
needed for the development of this work. M. P. gratefully acknowledges
Eric Feigelson for useful discussions and suggestions. P.L.G. thanks the
National Science Foundation through Grant No. AST-1009731 and the NASA
Astrophysics Theory Program through Grant No. NNX09AQ71G for their
generous support. The authors gratefully acknowledge the Pulsar Search
and Timing Consortia, all the radio scientists who contributed in
providing the radio light curves used in this paper, and the radio
observatories that generated the radio profiles used in this paper: the
Parkes Radio Telescope is part of the Australia Telescope which is
funded by the Commonwealth Government for operation as a National
Facility managed by CSIRO; the Green Bank Telescope is operated by the
National Radio Astronomy Observatory, a facility of the National Science
Foundation operated under cooperative agreement by Associated
Universities, Inc; the Arecibo Observatory is part of the National
Astronomy and Ionosphere Center (NAIC), a national research center
operated by Cornell University under a cooperative agreement with the
National Science Foundation; the Nancay Radio Observatory is operated by
the Paris Observatory, associated with the French Centre National de la
Recherche Scientifique (CNRS); the Lowe telescope is owned and operated
by the University of Manchester as part of the Jodrell Bank Centre for
Astrophysics with support from the Science and Technology Facilities
Council of the United Kingdom; the Westerbork Synthesis Radio Telescope
is operated by Netherlands Foundation for Radio Astronomy, ASTRON.
NR 26
TC 0
Z9 0
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2016
VL 588
AR A137
DI 10.1051/0004-6361/201527821
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0SQ
UT WOS:000373207800149
ER
PT J
AU Schulz, R
Kreikenbohm, A
Kadler, M
Ojha, R
Ros, E
Stevens, J
Edwards, PG
Carpenter, B
Elsasser, D
Gehrels, N
Grossberger, C
Hase, H
Horiuchi, S
Lovell, JEJ
Mannheim, K
Markowitz, A
Muller, C
Phillips, C
Plotz, C
Quick, J
Trustedt, J
Tzioumis, AK
Wilms, J
AF Schulz, R.
Kreikenbohm, A.
Kadler, M.
Ojha, R.
Ros, E.
Stevens, J.
Edwards, P. G.
Carpenter, B.
Elsaesser, D.
Gehrels, N.
Grossberger, C.
Hase, H.
Horiuchi, S.
Lovell, J. E. J.
Mannheim, K.
Markowitz, A.
Mueller, C.
Phillips, C.
Ploetz, C.
Quick, J.
Truestedt, J.
Tzioumis, A. K.
Wilms, J.
TI The gamma-ray emitting radio-loud narrow-line Seyfert 1 galaxy PKS
2004-447
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: individual: PKS 2004-447; radio continuum:
galaxies; techniques: interferometric; galaxies: jets
ID ACTIVE GALACTIC NUCLEI; COMPACT STEEP-SPECTRUM; LARGE-AREA TELESCOPE;
B3-VLA CSS SAMPLE; PMN J0948+0022; SOFTWARE CORRELATOR; VLBI
OBSERVATIONS; SCALE STRUCTURE; SOURCE CATALOG; SKY SURVEY
AB Context. Gamma-ray-detected radio-loud narrow-line Seyfert 1 (gamma-NLS1) galaxies constitute a small but interesting sample of the gamma-ray-loud AGN. The radio-loudest gamma-NLS1 known, PKS 2004 447, is located in the southern hemisphere and is monitored in the radio regime by the multiwavelength monitoring programme TANAMI.
Aims. We aim for the first detailed study of the radio morphology and long-term radio spectral evolution of PKS 2004 447, which are essential for understanding the diversity of the radio properties of gamma-NLS1s.
Methods. The TANAMI VLBI monitoring program uses the Australian Long Baseline Array (LBA) and telescopes in Antarctica, Chile, New Zealand, and South Africa to monitor the jets of radio-loud active galaxies in the southern hemisphere. Lower resolution radio flux density measurements at multiple radio frequencies over four years of observations were obtained with the Australia Telescope Compact Array (ATCA).
Results. The TANAMI VLBI image at 8.4 GHz shows an extended one-sided jet with a dominant compact VLBI core. Its brightness temperature is consistent with equipartition, but it is an order of magnitude below other gamma-NLS1s with the sample value varying over two orders of magnitude. We find a compact morphology with a projected large-scale size <11 kpc and a persistent steep radio spectrum with moderate flux-density variability.
Conclusions. PKS 2004 447 appears to be a unique member of the gamma-NLS1 sample. It exhibits blazar-like features, such as a flat featureless X-ray spectrum and a core-dominated, one-sided parsec-scale jet with indications for relativistic beaming. However, the data also reveal properties atypical for blazars, such as a radio spectrum and large-scale size consistent with compact-steep-spectrum (CSS) objects, which are usually associated with young radio sources. These characteristics are unique among all gamma-NLS1s and extremely rare among gamma-ray-loud AGN.
C1 [Schulz, R.; Kreikenbohm, A.; Kadler, M.; Elsaesser, D.; Mannheim, K.; Truestedt, J.] Univ Wurzburg, Lehrstuhl Astron, Campus Hubland Nord,Emil Fischer Str 31, D-97074 Wurzburg, Germany.
[Schulz, R.; Kreikenbohm, A.; Grossberger, C.; Markowitz, A.; Mueller, C.; Wilms, J.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, Sternwartstr 7, D-96049 Bamberg, Germany.
[Ojha, R.; Carpenter, B.; Gehrels, N.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Ojha, R.] Univ Maryland Baltimore Cty, 1000 Hilltop Cir, Baltimore, MD 21250 USA.
[Ojha, R.; Carpenter, B.] Catholic Univ Amer, 620 Michigan Ave NE, Washington, DC 20064 USA.
[Ros, E.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Ros, E.] Univ Valencia, Astron Observ, Paterna Valencia 46980, Spain.
[Ros, E.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
[Stevens, J.; Edwards, P. G.; Phillips, C.; Tzioumis, A. K.] CSIRO, Astron & Space Sci, ATNF, POB 76, Epping, NSW 1710, Australia.
[Grossberger, C.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85741 Garching, Germany.
[Hase, H.; Ploetz, C.] Bundesamt Kartog & Geodasie, D-93444 Bad Kotzingen, Germany.
[Horiuchi, S.] CSIRO Astron & Space Sci, Canberra Deep Space Commun Complex,POB 1035, Tuggeranong, ACT 2901, Australia.
[Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Private Bag 37, Hobart, Tas 7001, Australia.
[Markowitz, A.] Univ Calif San Diego, CASS, 9500 Gilman Dr,MC 0424, La Jolla, CA 92093 USA.
[Mueller, C.] Radboud Univ Nijmegen, Dept Astrophys, MAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Quick, J.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa.
RP Schulz, R (reprint author), Univ Wurzburg, Lehrstuhl Astron, Campus Hubland Nord,Emil Fischer Str 31, D-97074 Wurzburg, Germany.; Schulz, R (reprint author), Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, Sternwartstr 7, D-96049 Bamberg, Germany.
EM robert.schulz@physik.uni-wuerzburg.de
RI Wilms, Joern/C-8116-2013
OI Wilms, Joern/0000-0003-2065-5410
FU Deutsche Forschungsgemeinschaft [WI 1860/10-1]; Deutsches Zentrum fur
Luft- und Raumfahrt [50 OR 1303]; Spanish MINECO [AYA2009-13036-C02-02,
AYA2012-38491-C02-01]; Generalitat Valenciana [PROMETEO/2009/104,
PROMETEO/II/2014/057]; NASA [NNH09ZDA001N, NNH10ZDA001N, NNH12ZDA001N,
NNH13ZDA001N-FERMI, 31263, 41213, 61089, 71326]; Goddard Space Flight
Center; NASA; Commonwealth of Australia; [MP0905]
FX We thank the MPIfR internal referee S. Komossa and the anonymous journal
referee for their insightful comments, which improved the manuscript in
its final form. This work was funded by Deutsche Forschungsgemeinschaft
grant WI 1860/10-1. We acknowledge support by the Deutsches Zentrum fur
Luft- und Raumfahrt under contract number 50 OR 1303, by the Spanish
MINECO projects AYA2009-13036-C02-02 and AYA2012-38491-C02-01, and by
the Generalitat Valenciana projects PROMETEO/2009/104 and
PROMETEO/II/2014/057, as well as by the MP0905 action "Black Holes in a
Violent Universe". This research was funded in part by NASA through
Fermi Guest Investigator grants NNH09ZDA001N, NNH10ZDA001N,
NNH12ZDA001N, and NNH13ZDA001N-FERMI (proposal numbers 31263, 41213,
61089, and 71326, respectively). This research was supported by an
appointment to the NASA Postdoctoral Program at the Goddard Space Flight
Center, administered by Oak Ridge Associated Universities through a
contract with NASA. The Australian Long Baseline Array and the Australia
Telescope Compact Array are part of the Australia Telescope National
Facility, which is funded by the Commonwealth of Australia for operation
as a National Facility managed by CSIRO. This research made use of the
Interactive Spectral Interpretation System (ISIS) (Houck & Denicola
2000). This research made use of a collection of ISIS scripts provided
by the Dr. Karl Remeis observatory, Bamberg, Germany at http :
//www.sternwarte.uni-erlangen.de/isis/. This research made use of the
NASA /IPAC Extragalactic Database (NED), which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. This
research made use of the VizieR catalogue access tool, CDS, Strasbourg,
France. This research made use of data from the MOJAVE database that is
maintained by the MOJAVE team (Lister et al. 2009).
NR 81
TC 4
Z9 4
U1 1
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2016
VL 588
AR A146
DI 10.1051/0004-6361/201527404
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0SQ
UT WOS:000373207800158
ER
PT J
AU Tazzari, M
Testi, L
Ercolano, B
Natta, A
Isella, A
Chandler, CJ
Perez, LM
Andrews, S
Wilner, DJ
Ricci, L
Henning, T
Linz, H
Kwon, W
Corder, SA
Dullemond, CP
Carpenter, JM
Sargent, AI
Mundy, L
Storm, S
Calvet, N
Greaves, JA
Lazio, J
Deller, AT
AF Tazzari, M.
Testi, L.
Ercolano, B.
Natta, A.
Isella, A.
Chandler, C. J.
Perez, L. M.
Andrews, S.
Wilner, D. J.
Ricci, L.
Henning, T.
Linz, H.
Kwon, W.
Corder, S. A.
Dullemond, C. P.
Carpenter, J. M.
Sargent, A. I.
Mundy, L.
Storm, S.
Calvet, N.
Greaves, J. A.
Lazio, J.
Deller, A. T.
TI Multiwavelength analysis for interferometric (sub-)mm observations of
protoplanetary disks Radial constraints on the dust properties and the
disk structure
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; planetary systems; protoplanetary disks
ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; CIRCUMSTELLAR DISKS;
GRAIN-GROWTH; MILLIMETER WAVELENGTHS; OPTICAL-PROPERTIES; SIZE
DISTRIBUTION; TRANSITION DISK; ACCRETION DISKS; FORMING REGION
AB Context. The growth of dust grains from sub-mu m to mm and cm sizes is the first step towards the formation of planetesimals. Theoretical models of grain growth predict that dust properties change as a function of disk radius, mass, age, and other physical conditions. High angular resolution observations at several (sub-)mm wavelengths constitute the ideal tool with which to directly probe the bulk of dust grains and to investigate the radial distribution of their properties.
Aims. We lay down the methodology for a multiwavelength analysis of (sub-) mm and cm continuum interferometric observations to self-consistently constrain the disk structure and the radial variation of the dust properties. The computational architecture is massively parallel and highly modular.
Methods. The analysis is based on the simultaneous fit in the uv-plane of observations at several wavelengths with a model for the disk thermal emission and for the dust opacity. The observed flux density at the different wavelengths is fitted by posing constraints on the disk structure and on the radial variation of the grain size distribution.
Results. We apply the analysis to observations of three protoplanetary disks (AS 209, FT Tau, DR Tau) for which a combination of spatially resolved observations in the range similar to 0.88 mm to similar to 10 mm is available from SMA, CARMA, and VLA. In these disks we find evidence of a decrease in the maximum dust grain size, a(max), with radius. We derive large a(max) values up to 1 cm in the inner disk 15 AU <= R <= 30 AU and smaller grains with a(max) similar to 1 mm in the outer disk (R greater than or similar to 80 AU). Our analysis of the AS 209 protoplanetary disk confirms previous literature results showing a(max) decreasing with radius.
Conclusions. Theoretical studies of planetary formation through grain growth are plagued by the lack of direct information on the radial distribution of the dust grain size. In this paper we develop a multiwavelength analysis that will allow this missing quantity to be constrained for statistically relevant samples of disks and to investigate possible correlations with disk or stellar parameters.
C1 [Tazzari, M.; Testi, L.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Tazzari, M.; Testi, L.; Ercolano, B.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany.
[Testi, L.; Natta, A.] INAF Osservatorio Astrofis Arcetri, Largo Fermi 5, I-50125 Florence, Italy.
[Ercolano, B.] Univ Sternwarte Munchen, Scheinerstr 1, D-81679 Munich, Germany.
[Natta, A.] Dublin Inst Adv Studies, Sch Cosm Phys, 31 Fitzwilliam Pl, Dublin 2, Ireland.
[Isella, A.] Rice Univ, Dept Phys & Astron, 6100 Main St, Houston, TX 77005 USA.
[Chandler, C. J.; Perez, L. M.] Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA.
[Andrews, S.; Wilner, D. J.; Ricci, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Henning, T.; Linz, H.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Kwon, W.] Korea Astron & Space Sci Inst, 776 Daedeok Daero, Daejeon 34055, South Korea.
[Corder, S. A.] Joint ALMA Observ JAO, Ave Alonso de Cordova 3107, Santiago, Chile.
[Dullemond, C. P.] Heidelberg Univ, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany.
[Carpenter, J. M.; Sargent, A. I.] CALTECH, Dept Astron, MC 249-17, Pasadena, CA 91125 USA.
[Mundy, L.; Storm, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Calvet, N.] Univ Michigan, Dept Astron, 830 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA.
[Greaves, J. A.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Lazio, J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Deller, A. T.] Netherlands Inst Radio Astron ASTRON, NL-7990 Dwingeloo, Netherlands.
RP Tazzari, M (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.; Tazzari, M (reprint author), Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany.
EM mtazzari@eso.org
OI Tazzari, Marco/0000-0003-3590-5814; Deller, Adam/0000-0001-9434-3837
FU DFG cluster of excellence Origin and Structure of the Universe; NSF
[AST-1109334/1535809]; NASA Origins of Solar Systems program
[NNX14AD26G]; Italian Ministero dell' Istruzione, Universita e Ricerca
through Progetti Premiali - iALMA [CUP C52I13000140001]
FX M.T. and L.T. acknowledge support by the DFG cluster of excellence
Origin and Structure of the Universe (http://www.universe-cluster.de).
A. I. acknowledges support from the NSF award AST-1109334/1535809 and
from the NASA Origins of Solar Systems program through the award number
NNX14AD26G. The fits have been carried out on the computing facilities
of the Computational Center for Particle and Astrophysics (C2PAP) as
part of the approved project "Dust evolution in protoplanetary disks".
M.T. and L.T. are grateful for the experienced support from F. Beaujean
(C2PAP). M.T. thanks I. Jimenez-Serra, P. Papadopoulos, C. Manara and L.
Loreta for the precious support throughout this work. Figures have been
generated using the Python-based matplotlib package (Hunter 2007).
Staircase plots of PDFs have been generated with a user-modified version
of the Python-based triangle package (Foreman-Mackey et al. 2014). Plots
of the residuals have been generated with APLpy, an open-source plotting
package for Python hosted at http://aplpy.github.com. This research has
made use of the SIMBAD database, operated at CDS, Strasbourg, France.
This work was partly supported by the Italian Ministero dell'
Istruzione, Universita e Ricerca through the grant Progetti Premiali
2012 - iALMA (CUP C52I13000140001).
NR 82
TC 7
Z9 7
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2016
VL 588
AR A53
DI 10.1051/0004-6361/201527423
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0SQ
UT WOS:000373207800065
ER
PT J
AU Verdier, L
Melin, JB
Bartlett, JG
Magneville, C
Palanque-Delabrouille, N
Yeche, C
AF Verdier, Loic
Melin, Jean-Baptiste
Bartlett, James G.
Magneville, Christophe
Palanque-Delabrouille, Nathalie
Yeche, Christophe
TI Quasar host environments: The view from Planck
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE cosmology: observations; large-scale structure of Universe; quasars:
general; galaxies: clusters: general; methods: data analysis; methods:
statistical
ID ACTIVE GALACTIC NUCLEI; OSCILLATION SPECTROSCOPIC SURVEY; DIGITAL SKY
SURVEY; BARYON ACOUSTIC-OSCILLATIONS; SUPERMASSIVE BLACK-HOLES;
HIGH-REDSHIFT QUASARS; MM MAMBO/IRAM-30 M; SDSS-III; LUMINOSITY
FUNCTION; STAR-FORMATION
AB We measure the far-infrared emission of the general quasar (QSO) population using Planck observations of the Baryon Oscillation Spectroscopic Survey QSO sample. By applying multi-component matched multi-filters to the seven highest Planck frequencies, we extract the amplitudes of dust, synchrotron, and thermal Sunyaev-Zeldovich (SZ) signals for nearly 300 000 QSOs over the redshift range 0.1 < z < 5. We bin these individual low signal-to-noise measurements to obtain the mean emission properties of the QSO population as a function of redshift. The emission is dominated by dust at all redshifts, with a peak at z similar to 2, the same location as the peak in the general cosmic star formation rate. Restricting analysis to radio-loud QSOs, we find synchrotron emission with a monochromatic luminosity at 100 GHz (rest-frame) rising from (L-synch) over bar = 0 to 0.2 L-circle dot Hz(-1) between z = 0 and 3. The radio-quiet subsample does not show any synchrotron emission, but we detect thermal SZ between z = 2.5 and 4; no significant SZ emission is seen at lower redshifts. Depending on the supposed mass for the halos hosting the QSOs, this may or may not leave room for heating of the halo gas by feedback from the QSO.
C1 [Verdier, Loic; Melin, Jean-Baptiste; Magneville, Christophe; Palanque-Delabrouille, Nathalie; Yeche, Christophe] CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France.
[Bartlett, James G.] Univ Paris Diderot, AstroParticule & Cosmol, APC, CNRS,IN2P3,CEA,Irfu,Observ Paris,Sorbonne Paris C, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France.
[Bartlett, James G.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA.
RP Verdier, L; Melin, JB (reprint author), CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France.
EM loic.verdier@cea.fr; jean-baptiste.melin@cea.fr
FU National Aeronautics and Space Administration
FX Some of the results in this paper have been derived using the HEALPix
(Gorski et al. 2005) package. Part of this research was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration. We
thank T. Marriage for helpful discussions.
NR 81
TC 0
Z9 0
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2016
VL 588
AR A61
DI 10.1051/0004-6361/201527431
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0SQ
UT WOS:000373207800073
ER
PT J
AU Weiss, WW
Frohlich, HE
Pigulski, A
Popowicz, A
Huber, D
Kuschnig, R
Moffat, AFJ
Matthews, JM
Saio, H
Schwarzenberg-Czerny, A
Grant, CC
Koudelka, O
Luftinger, T
Rucinski, SM
Wade, GA
Alves, J
Guedel, M
Handler, G
Mochnacki, S
Orleanski, P
Pablo, B
Pamyatnykh, A
Ramiaramanantsoa, T
Rowe, J
Whittaker, G
Zawistowski, T
Zoclonska, E
Zwintz, K
AF Weiss, W. W.
Froehlich, H. -E.
Pigulski, A.
Popowicz, A.
Huber, D.
Kuschnig, R.
Moffat, A. F. J.
Matthews, J. M.
Saio, H.
Schwarzenberg-Czerny, A.
Grant, C. C.
Koudelka, O.
Lueftinger, T.
Rucinski, S. M.
Wade, G. A.
Alves, J.
Guedel, M.
Handler, G.
Mochnacki, St.
Orleanski, P.
Pablo, B.
Pamyatnykh, A.
Ramiaramanantsoa, T.
Rowe, J.
Whittaker, G.
Zawistowski, T.
Zoclonska, E.
Zwintz, K.
TI The roAp star alpha Circinus as seen by BRITE-Constellation
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: chemically peculiar; asteroseismology; stars: oscillations;
stars: rotation; stars: individual: alpha Cir; starspots
ID OSCILLATING AP STARS; PRECISION PHOTOMETRY; LIGHT VARIABILITY; H-ALPHA;
CIR; FREQUENCY; SPACE; SPECTROSCOPY; HD-128898; LINE
AB We report on an analysis of high-precision, multi-colour photometric observations of the rapidly-oscillating Ap (roAp) star alpha Cir. These observations were obtained with the BRITE-Constellation, which is a coordinated mission of five nanosatellites that collects continuous millimagnitude-precision photometry of dozens of bright stars for up to 180 days at a time in two colours (approximate to Johnson B and R). BRITE stands for BRight Target Explorer. The object alpha Cir is the brightest roAp star and an ideal target for such investigations, facilitating the determination of oscillation frequencies with high resolution. This star is bright enough for complementary interferometry and time-resolved spectroscopy. Four BRITE satellites observed alpha Cir for 146 d or 33 rotational cycles. Phasing the photometry according to the 4.4790 d rotational period reveals qualitatively different light variations in the two photometric bands. The phased red-band photometry is in good agreement with previously-published WIRE data, showing a light curve symmetric about phase 0.5 with a strong contribution from the first harmonic. The phased blue-lband data, in contrast, show an essentially sinusoidal variation. We model both light curves with Bayesian Photometric Imaging, which suggests the presence of two large-scale, photo-metrically bright (relative to the surrounding photosphere) spots. We also examine the high-frequency pulsation spectrum as encoded in the BRITE photometry. Our analysis establishes the stability of the main pulsation frequency over the last approximate to 20 yr, confirms the presence of frequency f(7), which was not detected (or the mode not excited) prior to 2006, and excludes quadrupolar modes for the main pulsation frequency.
C1 [Weiss, W. W.; Kuschnig, R.; Lueftinger, T.; Alves, J.; Guedel, M.] Univ Vienna, Inst Astrophys, Waehringer Guertel 18, A-1010 Vienna, Austria.
[Froehlich, H. -E.] Leibniz Inst Astrophys AIP, Kleine Str 9, D-14482 Potsdam, Germany.
[Pigulski, A.] Univ Wroclaw, Astron Inst, PL-50137 Wroclaw, Poland.
[Popowicz, A.] Silesian Tech Univ, Inst Automat Control, PL-44141 Gliwice, Poland.
[Moffat, A. F. J.; Pablo, B.; Ramiaramanantsoa, T.] Univ Montreal, Dept Phys, Montreal, PQ H3T 1J4, Canada.
[Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Grant, C. C.; Whittaker, G.] Univ Toronto, Space Flight Lab, Toronto, ON M5S, Canada.
[Huber, D.] Univ Sydney, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Huber, D.] SETI Inst, Mountain View, CA 94043 USA.
[Huber, D.] Aarhus Univ, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Koudelka, O.] Graz Univ Technol, A-8010 Graz, Austria.
[Saio, H.] Tohoku Univ, Astron Inst, Grad Sch Sci, Sendai, Miyagi 9808577, Japan.
[Schwarzenberg-Czerny, A.; Handler, G.; Pamyatnykh, A.; Zoclonska, E.] Nicolaus Copernicus Astron Ctr, Warsaw, Poland.
[Rucinski, S. M.; Mochnacki, St.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S, Canada.
[Orleanski, P.; Zawistowski, T.] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland.
[Rowe, J.] NASA, Ames Res Ctr, Montain View, CA 94035 USA.
[Wade, G. A.] Royal Mil Coll Canada, Dept Phys, Toronto, ON, Canada.
[Zwintz, K.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria.
RP Weiss, WW (reprint author), Univ Vienna, Inst Astrophys, Waehringer Guertel 18, A-1010 Vienna, Austria.; Frohlich, HE (reprint author), Leibniz Inst Astrophys AIP, Kleine Str 9, D-14482 Potsdam, Germany.; Pigulski, A (reprint author), Univ Wroclaw, Astron Inst, PL-50137 Wroclaw, Poland.
EM werner.weiss@univie.ac.at; hefroehlich@aip.de;
pigulski@astro.uni.wroc.pl
RI Guedel, Manuel/C-8486-2015
OI Guedel, Manuel/0000-0001-9818-0588
FU Austrian Science Funds (FWF); Austrian Research Promotion Agency
(FFG-ASAP); NSERC (Canada); FRQNT (Quebec); PMN grant
[2011/01/M/ST9/05914]; NCN grant [2011/03/B/ST9/02667]; Polish National
Science Center [2013/11/N/ST6/03051]; Polish NCN grant
[2011/01/B/ST9/05448]; Australian Research Council [DE140101364];
National Aeronautics and Space Administration [NNX14AB92G]; Austrian FFG
[ASAP11]; FWF NFN [S11601-N16, S116 604-N16]; Austrian Fonds zur
Forderung der wissenschaftlichen Forschung (FWF) [V431-NBL]
FX R.K. and W.W. were supported by the Austrian Science Funds (FWF) and by
the Austrian Research Promotion Agency (FFG-ASAP), which also supported
OK. A.F.J.M. is grateful for financial assistance from NSERC (Canada)
and FRQNT (Quebec). J.M.M., S.M.R., and G.A.W. are grateful for support
from NSERC (Canada). The Polish BRITE operations are funded by the PMN
grant 2011/01/M/ST9/05914. A.P.i. acknowledges the support from the NCN
grant No. 2011/03/B/ST9/02667 and APo was supported by the Polish
National Science Center, grant no. 2013/11/N/ST6/03051: Novel Methods of
Impulsive Noise Reduction in Astronomical Images. The MCMC computations
have been performed by HEF at the AIP. G.H. and A.P.a. received support
by the Polish NCN grant 2011/01/B/ST9/05448. D.H. acknowledges support
by the Australian Research Council's Discovery Projects funding scheme
(project number DE140101364) and support by the National Aeronautics and
Space Administration under Grant NNX14AB92G issued through the Kepler
Participating Scientist Program. T.L. acknowledges funding of the
Austrian FFG within ASAP11 and support by the FWF NFN projects
S11601-N16 and S116 604-N16. K.Z. acknowledges support by the Austrian
Fonds zur Forderung der wissenschaftlichen Forschung (FWF, project
V431-NBL). Finally, the authors wish to acknowledge the spacecraft
operation teams in Austria (P. Romano & M. Unterberger), Canada (Monica
Chaumont, Susan Choi, Daniel Kekez, Karan Sarda, Paul Choi & Laura
Bradbury) and Poland (Grzegorz Marciniszyn & Grzegorz Wozniak), whose
efforts were essential for the collection of the data used in this
paper.
NR 45
TC 1
Z9 1
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2016
VL 588
AR A54
DI 10.1051/0004-6361/201526997
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0SQ
UT WOS:000373207800066
ER
PT J
AU Yu, HF
Preece, RD
Greiner, J
Bhat, PN
Bissaldi, E
Briggs, MS
Cleveland, WH
Connaughton, V
Goldstein, A
von Kienlin, A
Kouveliotou, C
Mailyan, B
Meegan, CA
Paciesas, WS
Rau, A
Roberts, OJ
Veres, P
Wilson-Hodge, C
Zhang, BB
van Eerten, HJ
AF Yu, Hoi-Fung
Preece, Robert D.
Greiner, Jochen
Bhat, P. Narayana
Bissaldi, Elisabetta
Briggs, Michael S.
Cleveland, William H.
Connaughton, Valerie
Goldstein, Adam
von Kienlin, Andreas
Kouveliotou, Chryssa
Mailyan, Bagrat
Meegan, Charles A.
Paciesas, William S.
Rau, Arne
Roberts, Oliver J.
Veres, Peter
Wilson-Hodge, Colleen
Zhang, Bin-Bin
van Eerten, Hendrik J.
TI The Fermi GBM gamma-ray burst time-resolved spectral catalog: brightest
bursts in the first four years
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gamma rays: stars; gamma-ray burst: general; methods: data analysis
ID PROMPT EMISSION; BATSE OBSERVATIONS; PHOTOSPHERIC COMPONENT; NONTHERMAL
EMISSION; PEAK ENERGY; GRB 980923; MONITOR; TELESCOPE; EVOLUTION
AB Aims. We aim to obtain high-quality time-resolved spectral fits of gamma-ray bursts observed by the Gamma-ray Burst Monitor (GBM) on board the Fermi Gamma-ray Space Telescope.
Methods. We performed time-resolved spectral analysis with high temporal and spectral resolution of the brightest bursts observed by Fermi GBM in its first four years of mission.
Results. We present the complete catalog containing 1491 spectra from 81 bursts with high spectral and temporal resolution. Distributions of parameters, statistics of the parameter populations, parameter-parameter and parameter-uncertainty correlations, and their exact values are obtained and presented as main results in this catalog. We report a criterion that is robust enough to automatically distinguish between different spectral evolutionary trends between bursts. We also search for plausible blackbody emission components and find that only three bursts (36 spectra in total) show evidence of a pure Planck function. It is observed that peak energy and the averaged, time-resolved power-law index at low energy are slightly harder than the time-integrated values. Time-resolved spectroscopic results should be used instead of time-integrated results when interpreting physics from the observed spectra.
C1 [Yu, Hoi-Fung; Greiner, Jochen; von Kienlin, Andreas; Rau, Arne; van Eerten, Hendrik J.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Yu, Hoi-Fung; Greiner, Jochen] Tech Univ Munich, Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany.
[Preece, Robert D.] Univ Alabama, Dept Space Sci, Huntsville, AL 35809 USA.
[Bhat, P. Narayana; Briggs, Michael S.; Connaughton, Valerie; Mailyan, Bagrat; Veres, Peter; Zhang, Bin-Bin] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA.
[Bissaldi, Elisabetta] Ist Nazl Fis Nucl, Sez Bari, Via E Orabona 4, I-70125 Bari, Italy.
[Briggs, Michael S.; Connaughton, Valerie] Univ Alabama, Dept Phys, Huntsville, AL 35805 USA.
[Cleveland, William H.; Meegan, Charles A.; Paciesas, William S.] Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Goldstein, Adam; Wilson-Hodge, Colleen] NASA, Astrophys Off, Marshall Space Flight Ctr, ZP12, Huntsville, AL 35812 USA.
[Kouveliotou, Chryssa] George Washington Univ, Dept Phys, 725 21st St NW, Washington, DC 20052 USA.
[Roberts, Oliver J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
RP Yu, HF (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
EM sptfung@mpe.mpg.de
RI Bissaldi, Elisabetta/K-7911-2016; Roberts, Oliver/N-6284-2016
OI Bissaldi, Elisabetta/0000-0001-9935-8106; Roberts,
Oliver/0000-0002-7150-9061
FU DFG cluster of excellence "Origin and Structure of the Universe";
Science Foundation Ireland [12/IP/1288]; Alexander von Humboldt
foundation; German Bundesministeriums fur Wirtschaft und Technologie
(BMWi) via the Deutsches Zentrum fur Luft und Raumfahrt (DLR) [50 QV
0301, 50 OG 0502]
FX The authors wish to thank the anonymous referee for his/her insightful
comments. H.F.Y. and J.G. acknowledge support by the DFG cluster of
excellence "Origin and Structure of the Universe"
(www.universe-cluster.de). O.J.R. acknowledges support from Science
Foundation Ireland under Grant No. 12/IP/1288. H.J.v.E. acknowledges
support by the Alexander von Humboldt foundation. The GBM project is
supported by the German Bundesministeriums fur Wirtschaft und
Technologie (BMWi) via the Deutsches Zentrum fur Luft und Raumfahrt
(DLR) under the contract numbers 50 QV 0301 and 50 OG 0502.
NR 56
TC 1
Z9 1
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2016
VL 588
AR A135
DI 10.1051/0004-6361/201527509
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI0SQ
UT WOS:000373207800147
ER
PT J
AU Deary, AL
Metscher, B
Brill, RW
Hilton, EJ
AF Deary, Alison L.
Metscher, Brian
Brill, Richard W.
Hilton, Eric J.
TI Shifts of sensory modalities in early life history stage estuarine
fishes (Sciaenidae) from the Chesapeake Bay using X-ray micro computed
tomography
SO ENVIRONMENTAL BIOLOGY OF FISHES
LA English
DT Article
DE Drums; Ecomorphology; Ontogeny; Larvae; Foraging habitat; Brain
ID BRAIN-AREAS; FIBER-CONNECTIONS; INNER-EAR; SEBASTISCUS-MARMORATUS;
NAVODON-MODESTUS; MORPHOLOGY; TELEOST; TELENCEPHALON; ORGANIZATION;
PATTERNS
AB Increases in human populations along coasts have altered the estuarine nursery habitats that are important for many aquatic organisms. These perturbations include changes to the sensory environment due to increased turbidity resulting from runoff and nutrient loading; these changes are occurring faster than fish species can become adapted to the new prevailing conditions. However, understanding how modifications to the sensory environment impacts fishes during early life history stages (ELHS) requires understanding the senses used to locate food and evade predators and how they change during ontogeny. The drums (Sciaenidae) exhibit substantial morphological diversity in their peripheral sense organs as adults. We, therefore, used the relative volumes of their brain structures to assess ontogenetic changes in the sensory modalities of sciaenid species from different foraging guilds. Early stage sciaenids were imaged using X-ray micro computed tomography. The optic tract was the largest sensory region, suggesting that vision is the primary sensory modality in sciaenids, regardless of size, species, or foraging habitat. There were differences in the relative proportions of the other sensory areas according to foraging guild. These differences suggest that Cynoscion nebulosus (a pelagic forager) relies on audition and mechanoreception through ontogeny to augment vision, whereas Sciaenops ocellatus (a generalist forager) uses olfaction, audition, and mechanoreception. In contrast, Leiostomus xanthurus (a benthic forager) relies on olfaction and gustation. We propose that the ontogenetic trends in sensory modality described in sciaenids from the Chesapeake Bay (USA) can be used in future research to ascertain the potential species-specific impacts of water quality change on ELHS fishes.
C1 [Deary, Alison L.; Hilton, Eric J.] Virginia Inst Marine Sci, Coll William & Mary, POB 1346,1375 Greate Rd, Gloucester Point, VA 23690 USA.
[Metscher, Brian] Univ Vienna, Dept Theoret Biol, Althanstr 14, A-1090 Vienna, Austria.
[Brill, Richard W.] Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, James J Howard Marine Sci Lab, 74 Magruder Rd, Highlands, NJ 07732 USA.
[Deary, Alison L.] Univ So Mississippi, Gulf Coast Res Lab, Dept Coastal Sci, 703 East Beach Dr, Ocean Springs, MS 39564 USA.
RP Deary, AL (reprint author), Univ So Mississippi, Gulf Coast Res Lab, Dept Coastal Sci, 703 East Beach Dr, Ocean Springs, MS 39564 USA.
EM al.deary15@gmail.com
NR 52
TC 1
Z9 1
U1 2
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0378-1909
EI 1573-5133
J9 ENVIRON BIOL FISH
JI Environ. Biol. Fishes
PD APR
PY 2016
VL 99
IS 4
BP 361
EP 375
DI 10.1007/s10641-016-0479-8
PG 15
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA DK1KH
UT WOS:000374670500004
ER
PT J
AU Moffett, AJ
Ingarfield, SA
Driver, SP
Robotham, ASG
Kelvin, LS
Lange, R
Mestric, U
Alpaslan, M
Baldry, IK
Bland-Hawthorn, J
Brough, S
Cluver, ME
Davies, LJM
Holwerda, BW
Hopkins, AM
Kafle, PR
Kennedy, R
Norberg, P
Taylor, EN
AF Moffett, Amanda J.
Ingarfield, Stephen A.
Driver, Simon P.
Robotham, Aaron S. G.
Kelvin, Lee S.
Lange, Rebecca
Mestric, Uros
Alpaslan, Mehmet
Baldry, Ivan K.
Bland-Hawthorn, Joss
Brough, Sarah
Cluver, Michelle E.
Davies, Luke J. M.
Holwerda, Benne W.
Hopkins, Andrew M.
Kafle, Prajwal R.
Kennedy, Rebecca
Norberg, Peder
Taylor, Edward N.
TI Galaxy And Mass Assembly (GAMA): the stellar mass budget by galaxy type
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: fundamental
parameters; galaxies: luminosity function, mass function; galaxies:
spiral; galaxies: statistics
ID LUMINOSITY FUNCTION; REDSHIFT SURVEY; DISK GALAXIES; HUBBLE TYPE; SKY
SURVEY; ENVIRONMENT; EVOLUTION; IMPACT; SAMPLE; FIELD
AB We report an expanded sample of visual morphological classifications from the Galaxy and Mass Assembly survey phase two, which now includes 7556 objects (previously 3727 in phase one). We define a local (z < 0.06) sample and classify galaxies into E, S0-Sa, SB0-SBa, Sab-Scd, SBab-SBcd, Sd-Irr, and 'little blue spheroid' types. Using these updated classifications, we derive stellar mass function fits to individual galaxy populations divided both by morphological class and more general spheroid- or disc-dominated categories with a lower mass limit of log(M-*/M-aS (TM)) = 8 (one dex below earlier morphological mass function determinations). We find that all individual morphological classes and the combined spheroid-/bulge-dominated classes are well described by single Schechter stellar mass function forms. We find that the total stellar mass densities for individual galaxy populations and for the entire galaxy population are bounded within our stellar mass limits and derive an estimated total stellar mass density of rho(*) = 2.5 x 10(8) M-aS (TM) Mpc(-3) h(0.7), which corresponds to an approximately 4 per cent fraction of baryons found in stars. The mass contributions to this total stellar mass density by galaxies that are dominated by spheroidal components (E and S0-Sa classes) and by disc components (Sab-Scd and Sd-Irr classes) are approximately 70 and 30 per cent, respectively.
C1 [Moffett, Amanda J.; Ingarfield, Stephen A.; Driver, Simon P.; Robotham, Aaron S. G.; Lange, Rebecca; Davies, Luke J. M.; Kafle, Prajwal R.] Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia.
[Driver, Simon P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Kelvin, Lee S.; Mestric, Uros] Univ Innsbruck, Inst Astro & Teilchenphys, Technikerstr 25, A-6020 Innsbruck, Austria.
[Kelvin, Lee S.; Baldry, Ivan K.] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England.
[Alpaslan, Mehmet] NASA, Ames Res Ctr, N232, Mountain View, CA 94035 USA.
[Bland-Hawthorn, Joss] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Brough, Sarah; Hopkins, Andrew M.] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia.
[Cluver, Michelle E.] Univ Western Cape, Dept Phys, Robert Sobukwe Rd, ZA-7535 Bellville, South Africa.
[Holwerda, Benne W.] Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
[Kennedy, Rebecca] Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England.
[Norberg, Peder] Univ Durham, ICC, Dept Phys, Durham DH1 3LE, England.
[Norberg, Peder] Univ Durham, CEA, Dept Phys, Durham DH1 3LE, England.
[Taylor, Edward N.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia.
RP Moffett, AJ (reprint author), Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia.
EM amanda.moffett@uwa.edu.au
OI Alpaslan, Mehmet/0000-0003-0321-1033; Baldry, Ivan/0000-0003-0719-9385
FU Australian Research Council [130103505, FT140101166]; STFC (UK); ARC
(Australia); AAO; Alfred P. Sloan Foundation; National Science
Foundation; US Department of Energy; National Aeronautics and Space
Administration; Japanese Monbukagakusho; Max Planck Society; Higher
Education Funding Council for England; American Museum of Natural
History; Astrophysical Institute Potsdam; University of Basel;
University of Cambridge; Case Western Reserve University; University of
Chicago; Drexel University; Fermilab; Institute for Advanced Study;
Japan Participation Group; Johns Hopkins University; Joint Institute for
Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and
Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST);
Los Alamos National Laboratory; Max-Planck-Institute for Astronomy
(MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State
University; Ohio State University; University of Pittsburgh; University
of Portsmouth; Princeton University; United States Naval Observatory;
University of Washington; ESO Telescopes at the La Silla Paranal
Observatory under the programme [179.A-2004]
FX SPD and AJM acknowledge funding support from the Australian Research
Council under Discovery Project grant 130103505. SB acknowledges funding
support from the Australian Research Council through a Future Fellowship
(FT140101166).; GAMA is a joint European-Australasian project based
around a spectroscopic campaign using the Anglo-Australian Telescope.
The GAMA input catalogue is based on data taken from the SDSS and the
UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA
regions is being obtained by a number of independent survey programmes
including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT,
and ASKAP providing UV to radio coverage. GAMA is funded by the STFC
(UK), the ARC (Australia), the AAO, and the participating institutions.
The GAMA website is http://www.gama-survey.org/.; Funding for the SDSS
and SDSS-II has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, the US
Department of Energy, the National Aeronautics and Space Administration,
the Japanese Monbukagakusho, the Max Planck Society, and the Higher
Education Funding Council for England. The SDSS WebSite is
http://www.sdss.org/. The SDSS is managed by the Astrophysical Research
Consortium for the Participating Institutions. The Participating
Institutions are the American Museum of Natural History, Astrophysical
Institute Potsdam, University of Basel, University of Cambridge, Case
Western Reserve University, University of Chicago, Drexel University,
Fermilab, the Institute for Advanced Study, the Japan Participation
Group, Johns Hopkins University, the Joint Institute for Nuclear
Astrophysics, the Kavli Institute for Particle Astrophysics and
Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences
(LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for
Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New
Mexico State University, Ohio State University, University of
Pittsburgh, University of Portsmouth, Princeton University, the United
States Naval Observatory, and the University of Washington.; The VIKING
survey is based on observations with ESO Telescopes at the La Silla
Paranal Observatory under the programme ID 179.A-2004.
NR 59
TC 12
Z9 12
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 1
PY 2016
VL 457
IS 2
BP 1308
EP 1319
DI 10.1093/mnras/stv2883
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6AB
UT WOS:000373580500015
ER
PT J
AU Ventura, P
Karakas, AI
Dell'Agli, F
Garcia-Hernandez, DA
Boyer, ML
Di Criscienzo, M
AF Ventura, P.
Karakas, A. I.
Dell'Agli, F.
Garcia-Hernandez, D. A.
Boyer, M. L.
Di Criscienzo, M.
TI On the nature of the most obscured C-rich AGB stars in the Magellanic
Clouds
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: abundances; stars: AGB and post-AGB; Magellanic Clouds
ID ASYMPTOTIC GIANT BRANCH; 3RD DREDGE-UP; COLOR-MAGNITUDE DIAGRAMS;
INTERMEDIATE-MASS STARS; DUST FORMATION; GALAXY EVOLUTION;
LOW-METALLICITY; EVOLVED STARS; CARBON STARS; STELLAR WINDS
AB The stars in the Magellanic Clouds with the largest degree of obscuration are used to probe the highly uncertain physics of stars in the asymptotic giant branch (AGB) phase of evolution. Carbon stars in particular provide key information on the amount of third dredge-up and mass-loss. We use two independent stellar evolution codes to test how a different treatment of the physics affects the evolution on the AGB. The output from the two codes is used to determine the rates of dust formation in the circumstellar envelope, where the method used to determine the dust is the same for each case. The stars with the largest degree of obscuration in the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) are identified as the progeny of objects of initial mass 2.5-3 M-aS (TM) and similar to 1.5 M-aS (TM), respectively. This difference in mass is motivated by the difference in the star formation histories of the two galaxies, and offers a simple explanation of the redder infrared colours of C-stars in the LMC compared to their counterparts in the SMC. The comparison with the Spitzer colours of C-rich AGB stars in the SMC shows that a minimum surface carbon mass fraction X(C) similar to 5 x 10(-3) must have been reached by stars of initial mass around 1.5 M-aS (TM). Our results confirm the necessity of adopting low-temperature opacities in stellar evolutionary models of AGB stars. These opacities allow the stars to obtain mass-loss rates high enough (a parts per thousand(3)10(-4) M-aS (TM) yr(-1)) to produce the amount of dust needed to reproduce the Spitzer colours.
C1 [Ventura, P.; Dell'Agli, F.; Di Criscienzo, M.] INAF Osservatorio Astronom Roma, Via Frascati 33,00040, I-00077 Monte Porzio Catone, RM, Italy.
[Karakas, A. I.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Karakas, A. I.] Monash Univ, Sch Phys & Astron, Monash Ctr Astrophys, Clayton, Vic 3800, Australia.
[Garcia-Hernandez, D. A.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Garcia-Hernandez, D. A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
[Boyer, M. L.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Boyer, M. L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Ventura, P (reprint author), INAF Osservatorio Astronom Roma, Via Frascati 33,00040, I-00077 Monte Porzio Catone, RM, Italy.
EM paolo.ventura@oa-roma.inaf.it
FU PRIN MIUR [2010LY5N2T]; Australian Research Council [FT110100475]; Ramon
y Cajal fellowship [RYC-2013-14182]; Spanish Ministry of Economy and
Competitiveness (MINECO) [AYA-2014-58082-P]; Observatory of Rome
FX The authors are indebted to the referee, J. Th. van Loon, for the
careful reading of the manuscript and for the several comments, which
help improving significantly the quality of this work. PV was supported
by PRIN MIUR 2011 'The Chemical and Dynamical Evolution of the Milky Way
and Local Group Galaxies' (PI: F. Matteucci), prot. 2010LY5N2T. AIK was
supported through an Australian Research Council Future Fellowship
(FT110100475). DAGH was funded by the Ramon y Cajal fellowship number
RYC-2013-14182 and he acknowledges support provided by the Spanish
Ministry of Economy and Competitiveness (MINECO) under grant
AYA-2014-58082-P. FD and MDC acknowledge support from the Observatory of
Rome.
NR 84
TC 6
Z9 6
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 1
PY 2016
VL 457
IS 2
BP 1456
EP 1467
DI 10.1093/mnras/stw074
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6AB
UT WOS:000373580500028
ER
PT J
AU Cohn, JD
White, M
Chang, TC
Holder, G
Padmanabhan, N
Dore, O
AF Cohn, J. D.
White, Martin
Chang, Tzu-Ching
Holder, Gil
Padmanabhan, Nikhil
Dore, Olivier
TI Combining galaxy and 21-cm surveys
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitation; galaxies: statistics; cosmological parameters; large-scale
structure of Universe
ID BARYON ACOUSTIC-OSCILLATIONS; ZELDOVICH APPROXIMATION; 2-POINT
CORRELATION; REDSHIFT SPACE; SCALE; RECONSTRUCTION; INTERFEROMETRY;
COSMOLOGY; DISTANCE; QUASARS
AB Acoustic waves travelling through the early Universe imprint a characteristic scale in the clustering of galaxies, QSOs and intergalactic gas. This scale can be used as a standard ruler to map the expansion history of the Universe, a technique known as baryon acoustic oscillations (BAO). BAO offer a high-precision, low-systematics means of constraining our cosmological model. The statistical power of BAO measurements can be improved if the 'smearing' of the acoustic feature by non-linear structure formation is undone in a process known as reconstruction. In this paper, we use low-order Lagrangian perturbation theory to study the ability of 21-cm experiments to perform reconstruction and how augmenting these surveys with galaxy redshift surveys at relatively low number densities can improve performance. We find that the critical number density which must be achieved in order to benefit 21-cm surveys is set by the linear theory power spectrum near its peak, and corresponds to densities achievable by upcoming surveys of emission line galaxies such as eBOSS and DESI. As part of this work, we analyse reconstruction within the framework of Lagrangian perturbation theory with local Lagrangian bias, redshift-space distortions, k-dependent noise and anisotropic filtering schemes.
C1 [Cohn, J. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Cohn, J. D.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA.
[White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[White, Martin] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
[White, Martin] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA.
[Chang, Tzu-Ching] Acad Sinica, ASMAB 11F, AS NTU, Inst Astron & Astrophys, 1 Roosevelt Rd Sect 4, Taipei 10617, Taiwan.
[Holder, Gil] McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada.
[Padmanabhan, Nikhil] Yale Univ, Dept Phys, New Haven, CT 06511 USA.
[Dore, Olivier] CALTECH, MC 350-17, Pasadena, CA 91125 USA.
[Dore, Olivier] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA.
RP Cohn, JD (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.; Cohn, JD (reprint author), Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA.
EM jcohn@berkeley.edu
RI White, Martin/I-3880-2015
OI White, Martin/0000-0001-9912-5070
FU National Science Foundation [PHY-1066293]; MoST [103-2112-M-001-002-MY3]
FX We would like to thank Marcel Schmittfull for helpful conversations on
acoustic oscillations and reconstruction, and Josh Dillon, Daniel
Eisenstein, Marcel Schmittfull, Uros Seljak and Hee-Jong Seo for helpful
feedback on the draft, and the anonymous referee for additional helpful
suggestions. This work was begun at the Aspen Center for Physics, which
is supported by National Science Foundation grant PHY-1066293. We thank
the Center for its hospitality. T-CC acknowledges support from MoST
grant 103-2112-M-001-002-MY3. This work made extensive use of the NASA
Astrophysics Data System and of the astro-ph preprint archive at
arXiv.org.
NR 53
TC 4
Z9 4
U1 1
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 1
PY 2016
VL 457
IS 2
BP 2068
EP 2077
DI 10.1093/mnras/stw108
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6AB
UT WOS:000373580500073
ER
PT J
AU Cook, NJ
Pinfield, DJ
Marocco, F
Burningham, B
Jones, HRA
Frith, J
Zhong, J
Luo, AL
Qi, ZX
Lucas, PW
Gromadzki, M
Day-Jones, AC
Kurtev, RG
Guo, YX
Wang, YF
Bai, Y
Yi, ZP
Smart, RL
AF Cook, N. J.
Pinfield, D. J.
Marocco, F.
Burningham, B.
Jones, H. R. A.
Frith, J.
Zhong, J.
Luo, A. L.
Qi, Z. X.
Lucas, P. W.
Gromadzki, M.
Day-Jones, A. C.
Kurtev, R. G.
Guo, Y. X.
Wang, Y. F.
Bai, Y.
Yi, Z. P.
Smart, R. L.
TI A method for selecting M dwarfs with an increased likelihood of
unresolved ultracool companionship
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: observational; brown dwarfs; stars: low-mass; infrared: stars
ID DIGITAL SKY SURVEY; LOW-MASS STARS; EXTRASOLAR GIANT PLANETS;
INFRARED-SURVEY-EXPLORER; BROWN DWARFS; T-DWARFS; SURVEY 2MASS;
RADIAL-VELOCITIES; DATA RELEASE; FIELD
AB Locating ultracool companions to M dwarfs is important for constraining low-mass formation models, the measurement of substellar dynamical masses and radii, and for testing ultracool evolutionary models. We present an optimized method for identifying M dwarfs which may have unresolved ultracool companions. We construct a catalogue of 440 694 M dwarf candidates, from Wide-Field Infrared Survey Explorer, Two Micron All-Sky Survey and Sloan Digital Sky Survey, based on optical- and near-infrared colours and reduced proper motion. With strict reddening, photometric and quality constraints we isolate a subsample of 36 898 M dwarfs and search for possible mid-infrared M dwarf + ultracool dwarf candidates by comparing M dwarfs which have similar optical/near-infrared colours (chosen for their sensitivity to effective temperature and metallicity). We present 1082 M dwarf + ultracool dwarf candidates for follow-up. Using simulated ultracool dwarf companions to M dwarfs, we estimate that the occurrence of unresolved ultracool companions amongst our M dwarf + ultracool dwarf candidates should be at least four times the average for our full M dwarf catalogue. We discuss possible contamination and bias and predict yields of candidates based on our simulations.
C1 [Cook, N. J.; Pinfield, D. J.; Marocco, F.; Burningham, B.; Jones, H. R. A.; Frith, J.; Lucas, P. W.; Day-Jones, A. C.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Burningham, B.] NASA, Ames Res Ctr, Mail Stop 245-3, Moffett Field, CA 94035 USA.
[Zhong, J.; Qi, Z. X.] Chinese Acad Sci, SHAO, Key Lab Res Galaxies & Cosmol, 80 Nandan Rd, Shanghai 200030, Peoples R China.
[Luo, A. L.; Guo, Y. X.; Wang, Y. F.; Bai, Y.] Chinese Acad Sci, NAO, Key Lab Opt Astron, Datun Rd 20A, Beijing 100012, Peoples R China.
[Gromadzki, M.; Kurtev, R. G.] Millennium Inst Astrophys, Av Vicua Mackenna 4860, Santiago 7820436, Chile.
[Gromadzki, M.; Kurtev, R. G.] Univ Valparaiso, Ist Fis & Astron, Ave Gran Bretana 1111,Casilla 5030, Valparaiso, Chile.
[Yi, Z. P.] Shandong Univ, Weihai 264209, Peoples R China.
[Smart, R. L.] Ist Nazl Astrofis, Osservatorio Astron Torino, Via Osservatorio, I-10023 Turin, Italy.
RP Cook, NJ (reprint author), Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
EM neil.james.cook@gmail.com
OI cook, Neil/0000-0003-4166-4121; Burningham, Ben/0000-0003-4600-5627;
Jones, Hugh/0000-0003-0433-3665
FU UK's Science and Technology Facilities Council [ST/K502091/1]; Marie
Curie 7th European Community Framework Programme [247593]; Joined
Committee ESO; Government of Chile; Fondecyt Regular [1120601, 1130140];
Ministry for the Economy, Development, and Tourisms Programa Inicativa
Cientifica Milenio [IC 12009, 140042]; NASA; 2MASS; NSF; Alfred P. Sloan
Foundation; USDOESC; National Development and Reform Commission
FX NJC acknowledges support from the UK's Science and Technology Facilities
Council [grant number ST/K502091/1], and has benefited from IPERCOOL,
grant number 247593 within the Marie Curie 7th European Community
Framework Programme. MG acknowledges support from Joined Committee ESO
and Government of Chile 2014 and Fondecyt Regular No. 1120601. Support
for MG and RGK is provided by the Ministry for the Economy, Development,
and Tourisms Programa Inicativa Cientifica Milenio through grant IC
12009, awarded to The Millennium Institute of Astrophysics (MAS) and
acknowledgement to CONICYT REDES No. 140042 project. RGK is supported by
Fondecyt Regular No. 1130140. We make use of data products from WISE
(Wright et al. 2010), which is a joint project of the UCLA, and the
JPL/CIT, funded by NASA, and 2MASS (Skrutskie et al. 2006), which is a
joint project of the University of Massachusetts and the Infrared
Processing and Analysis Center/CIT, funded by NASA and the NSF. We also
make substantial use of SDSS DR10, funding for SDSS-III has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the NSF, and the USDOESC. This research has made use of
the NASA/IPAC Infrared Science Archive1, which is operated by
JPL, CIT, under contract with NASA, and the VizieR data base catalogue
access tool and SIMBAD data base of Wenger et al. (2000), operated at
CDS, Strasbourg, France. This work is based in part on services provided
by the GAVO Data Center and the data products from the PPMXL data base
of Roeser et al. (2010). This publication has made use of LAMOST DR1 and
DR2 spectra. Guoshoujing Telescope (LAMOST) is a National Major
Scientific Project built by CAS. Funding for the project has been
provided by the National Development and Reform Commission. LAMOST is
operated and managed by the NAO, CAS. This research has benefited from
the SpeX Prism Spectral Libraries, maintained by Adam
Burgasser13. This research made extensive use of ASTROPY
(Astropy Collaboration et al. 2013), MATPLOTLIB (Chabrier, Gallardo &
Baraffe 2007), SCIPY (Jones et al. 2001), TOPCAT (Taylor 2005), STILTS
(Taylor 2006), IPYTHON (Perez & Granger 2007), and NASA's Astrophysics
Data System.
NR 90
TC 0
Z9 0
U1 2
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 1
PY 2016
VL 457
IS 2
BP 2192
EP 2208
DI 10.1093/mnras/stw061
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6AB
UT WOS:000373580500082
ER
PT J
AU Spingola, C
Dallacasa, D
Orienti, M
Giroletti, M
McKean, JP
Cheung, CC
Hovatta, T
Ciprini, S
D'Ammando, F
Falco, E
Larsson, S
Max-Moerbeck, W
Ojha, R
Readhead, ACS
Richards, JL
Scargle, J
AF Spingola, C.
Dallacasa, D.
Orienti, M.
Giroletti, M.
McKean, J. P.
Cheung, C. C.
Hovatta, T.
Ciprini, S.
D'Ammando, F.
Falco, E.
Larsson, S.
Max-Moerbeck, W.
Ojha, R.
Readhead, A. C. S.
Richards, J. L.
Scargle, J.
TI Radio follow-up of the gamma-ray flaring gravitational lens JVAS
B0218+357
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: strong; quasars: individual: JVAS B0218+357
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; BLAZAR PKS 1830-211;
ALL-SKY SURVEY; SUPERLUMINAL MOTION; SYSTEM B0218+357; BRIGHT BLAZARS;
EINSTEIN RING; TIME-DELAY; VARIABILITY
AB We present results on multifrequency Very Long Baseline Array (VLBA) monitoring observations of the double-image gravitationally lensed blazar JVAS B0218+357. Multi-epoch observations started less than one month after the gamma-ray flare detected in 2012 by the Large Area Telescope on board Fermi, and spanned a 2-month interval. The radio light curves did not reveal any significant flux density variability, suggesting that no clear correlation between the high-energy and low-energy emission is present. This behaviour was confirmed also by the long-term Owens Valley Radio Observatory monitoring data at 15 GHz. The milliarcsecond-scale resolution provided by the VLBA observations allowed us to resolve the two images of the lensed blazar, which have a core-jet structure. No significant morphological variation is found by the analysis of the multi-epoch data, suggesting that the region responsible for the gamma-ray variability is located in the core of the active galactic nuclei, which is opaque up to the highest observing frequency of 22 GHz.
C1 [Spingola, C.; Dallacasa, D.; D'Ammando, F.] Univ Bologna, Dipartmento Astron, Via Ranzani 1, I-40127 Bologna, Italy.
[Spingola, C.; Dallacasa, D.; Orienti, M.; Giroletti, M.; D'Ammando, F.] INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy.
[Spingola, C.; McKean, J. P.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
[McKean, J. P.] Netherlands Inst Radio Astron ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands.
[Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Hovatta, T.] Aalto Univ Metsahovi Radio Observ, Metsahovintie 114, FI-02540 Kylmala, Finland.
[Ciprini, S.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy.
[Ciprini, S.] Ist Nazl Astrofis, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Roma, Italy.
[Falco, E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Larsson, S.] KTH Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden.
[Larsson, S.] AlbaNova, Oscar Klein Ctr, SE-10691 Stockholm, Sweden.
[Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Max-Moerbeck, W.] Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA.
[Ojha, R.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Ojha, R.] Univ Maryland Baltimore Cty, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Ojha, R.] Catholic Univ Amer, 620 Michigan Ave NE, Washington, DC 20064 USA.
[Readhead, A. C. S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Richards, J. L.] Purdue Univ, Dept Phys & Astron, 525 Northwestern Ave, W Lafayette, IN 47907 USA.
[Scargle, J.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Spingola, C; Dallacasa, D (reprint author), Univ Bologna, Dipartmento Astron, Via Ranzani 1, I-40127 Bologna, Italy.; Spingola, C; Dallacasa, D; Orienti, M (reprint author), INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy.; Spingola, C (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
EM spingola@astro.rug.nl; ddallaca@ira.inaf.it; orienti@ira.inaf.it
OI Spingola, Cristiana/0000-0002-2231-6861
FU National Aeronautics and Space Administration; NASA Guest Investigator
programme [13-FERMI13-0009]; Royal Swedish Academy Crafoord Foundation;
NASA [NNX08AW31G, NNX11A043G]; NSF [AST-0808050, AST-1109911]; NASA
through Fermi Guest Investigator grants [NNH09ZDA001N, NNH10ZDA001N,
NNH12ZDA001N, NNH13ZDA001N-FERMI]
FX The VLBA is operated by the US National Radio Astronomy Observatory
which is a facility of the National Science Foundation operated under a
cooperative agreement by Associated University, Inc., under contract
with the National Science Foundation. This research has made use of the
NASA/IPAC Extragalactic Database (NED), which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.; CCC
was supported at NRL by NASA Guest Investigator programme
13-FERMI13-0009. SL was supported by the Royal Swedish Academy Crafoord
Foundation. We thank the NRAO Schedsoc for approving our request and
Mark Claussen for facilitating the VLBA scheduling. The OVRO 40-m
monitoring programme is supported in part by NASA grants NNX08AW31G and
NNX11A043G, and NSF grants AST-0808050 and AST-1109911.; This research
was funded in part by NASA through Fermi Guest Investigator grants
NNH09ZDA001N, NNH10ZDA001N, NNH12ZDA001N, NNH13ZDA001N-FERMI. This
research was supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA.
NR 44
TC 4
Z9 4
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 1
PY 2016
VL 457
IS 2
BP 2263
EP 2271
DI 10.1093/mnras/stw136
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI6AB
UT WOS:000373580500086
ER
PT J
AU France, K
Loyd, ROP
Youngblood, A
Brown, A
Schneider, PC
Hawley, SL
Froning, CS
Linsky, JL
Roberge, A
Buccino, AP
Davenport, JRA
Fontenla, JM
Kaltenegger, L
Kowalski, AF
Mauas, PJD
Miguel, Y
Redfield, S
Rugheimer, S
Tian, F
Vieytes, MC
Walkowicz, LM
Weisenburger, KL
AF France, Kevin
Loyd, R. O. Parke
Youngblood, Allison
Brown, Alexander
Schneider, P. Christian
Hawley, Suzanne L.
Froning, Cynthia S.
Linsky, Jeffrey L.
Roberge, Aki
Buccino, Andrea P.
Davenport, James R. A.
Fontenla, Juan M.
Kaltenegger, Lisa
Kowalski, Adam F.
Mauas, Pablo J. D.
Miguel, Yamila
Redfield, Seth
Rugheimer, Sarah
Tian, Feng
Vieytes, Mariela C.
Walkowicz, Lucianne M.
Weisenburger, Kolby L.
TI THE MUSCLES TREASURY SURVEY. I. MOTIVATION AND OVERVIEW
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: activity; stars: low-mass
ID LOCAL INTERSTELLAR-MEDIUM; HUBBLE-SPACE-TELESCOPE; LOW-MASS STAR;
POTENTIALLY HABITABLE PLANETS; EXTRASOLAR GIANT PLANETS; EXOPLANET HOST
STARS; MAIN-SEQUENCE STARS; EARTH-LIKE PLANETS; GJ 436 SYSTEM; M-DWARF
STARS
AB Ground-and space-based planet searches employing radial velocity techniques and transit photometry have detected thousands of planet-hosting stars in the Milky Way. With so many planets discovered, the next step toward identifying potentially habitable planets is atmospheric characterization. While the Sun-Earth system provides a good framework for understanding the atmospheric chemistry of Earth-like planets around solar-type stars, the observational and theoretical constraints on the atmospheres of rocky planets in the habitable zones (HZs) around low-mass stars (K and M dwarfs) are relatively few. The chemistry of these atmospheres is controlled by the shape and absolute flux of the stellar spectral energy distribution (SED), however, flux distributions of relatively inactive low-mass stars are poorly understood at present. To address this issue, we have executed a panchromatic (X-ray to mid-IR) study of the SEDs of 11 nearby planet-hosting stars, the Measurements of the Ultraviolet Spectral Characteristics of Low-mass Exoplanetary Systems (MUSCLES) Treasury Survey. The MUSCLES program consists visible observations from Hubble and ground-based observatories. Infrared and astrophysically inaccessible wavelengths (EUV and Ly alpha) are reconstructed using stellar model spectra to fill in gaps in the observational data. In this overview and the companion papers describing the MUSCLES survey, we show that energetic radiation (X-ray and ultraviolet) is present from magnetically active stellar atmospheres at all times for stars as late as M6. The emission line luminosities of C IV and Mg II are strongly correlated with band-integrated luminosities and we present empirical relations that can be used to estimate broadband FUV and XUV (equivalent to X-ray + EUV) fluxes from individual stellar emission line measurements. We find that while the slope of the SED, FUV/NUV, increases by approximately two orders of magnitude form early K to late M dwarfs (approximate to 0.01-1), the absolute FUV and XUV flux levels at their corresponding HZ distances are constant to within factors of a few, spanning the range 10-70 erg cm(-2) s(-1) in the HZ. Despite the lack of strong stellar activity indicators in their optical spectra, several of the M dwarfs in our sample show spectacular UV flare emission in their light curves. We present an example with flare/quiescent ultraviolet flux ratios of the order of 100:1 where the transition region energy output during the flare is comparable to the total quiescent luminosity of the star E-flare(UV) similar to 0.3 L-*Delta t (Delta t = 1 s). Finally, we interpret enhanced L(line)/L-Bol ratios for C IV and N V as tentative observational evidence for the interaction of planets with large planetary mass-to-orbital distance ratios (M-plan/a(plan)) with the transition regions of their host stars.
C1 [France, Kevin; Loyd, R. O. Parke; Youngblood, Allison] Univ Colorado, Lab Atmospher & Space Phys, 600 UCB, Boulder, CO 80309 USA.
[Brown, Alexander] Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA.
[Schneider, P. Christian] European Space Res & Technol Ctr ESA ESTEC, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
[Hawley, Suzanne L.; Weisenburger, Kolby L.] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
[Froning, Cynthia S.] Univ Texas Austin, Dept Astron, C1400, Austin, TX 78712 USA.
[Linsky, Jeffrey L.] Univ Colorado, JILA, 440 UCB, Boulder, CO 80309 USA.
[Linsky, Jeffrey L.] NIST, 440 UCB, Boulder, CO 80309 USA.
[Roberge, Aki] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Buccino, Andrea P.; Mauas, Pablo J. D.; Vieytes, Mariela C.] Inst Astron & Fis Espacio UBA CONICET, CC 67,Suc 28, RA-1428 Buenos Aires, DF, Argentina.
[Buccino, Andrea P.; Mauas, Pablo J. D.] Dept Fis UBA, CC 67,Suc 28, RA-1428 Buenos Aires, DF, Argentina.
[Davenport, James R. A.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA.
[Fontenla, Juan M.] North West Res Associates, 3380 Mitchell Lane, Boulder, CO 80301 USA.
[Kaltenegger, Lisa] Cornell Univ, Carl Sagan Inst, Ithaca, NY 14850 USA.
[Kowalski, Adam F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Miguel, Yamila] Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS, Lab Lagrange, Blvd Observ,CS 34229, F-06304 Nice 4, France.
[Redfield, Seth] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA.
[Redfield, Seth] Wesleyan Univ, Van Vleck Observ, Middletown, CT 06459 USA.
[Rugheimer, Sarah] Univ St Andrews, Dept Earth & Environm Sci, Irvine Bldg, St Andrews KY16 9AL, Fife, Scotland.
[Tian, Feng] Tsinghua Univ, Ctr Earth Syst Sci, Key Lab Earth Syst Modeling, Minist Educ, Beijing 100084, Peoples R China.
[Vieytes, Mariela C.] UNTREF, CC 67,Suc 28, RA-1428 Buenos Aires, DF, Argentina.
[Walkowicz, Lucianne M.] Adler Planetarium, 1300 S Lakeshore Dr, Chicago, IL 60605 USA.
RP France, K (reprint author), Univ Colorado, Lab Atmospher & Space Phys, 600 UCB, Boulder, CO 80309 USA.
EM kevin.france@colorado.edu
RI Tian, Feng/C-1344-2015;
OI Tian, Feng/0000-0002-9607-560X; Rugheimer, Sarah/0000-0003-1620-7658;
Redfield, Seth/0000-0003-3786-3486; FRANCE, KEVIN/0000-0002-1002-3674;
Roberge, Aki/0000-0002-2989-3725
FU HST Guest Observing programs [12464, 13650]; COS Science Team Guaranteed
Time programs [12034, 12035]; STScI [HST-GO-12464.01, HST-GO-13650.01];
Smithsonian Astrophysical Observatory [GO4-15014X, GO5-16155X]; NASA
[NNX16AC09G]; NSF [AST 13-11678]; National Natural Science Foundation of
China [41175039]; Ministry of Education of China [20131029170]; Tsinghua
University Initiative Scientific Research Program; ESA Research
Fellowship
FX The data presented here were obtained as part of the HST Guest Observing
programs #12464 and #13650 as well as the COS Science Team Guaranteed
Time programs # 12034 and # 12035. This work was supported by STScI
grants HST-GO-12464.01 and HST-GO-13650.01 to the University of Colorado
at Boulder. Data for the MUSCLES Treasury Survey were also acquired as
part of Chandra and XMM guest observing programs, supported by Chandra
grants GO4-15014X and GO5-16155X from the Smithsonian Astrophysical
Observatory and NASA XMM grant NNX16AC09G to the University of Colorado
at Boulder. This work is based in part upon observations obtained with
the Apache Point Observatory 3.5 m and 0.5 m telescopes, which are owned
and operated by the Astrophysical Research Consortium. K.F. thanks
Evgenya Shkolnik for enjoyable discussions about low-mass stars and
Jorge Sanz-Forcada for assistance with the absolute flux levels of the
X-exoplanets model spectra. The MUSCLES team also thanks STScI program
coordinator Amber Armstrong for her long hours spent scheduling these
complicated coordinated observations. P.C.S. gratefully acknowledges an
ESA Research Fellowship. S.L.H. acknowledges support from NSF grant AST
13-11678. F.T. is supported by the National Natural Science Foundation
of China (41175039), the Startup Fund of the Ministry of Education of
China (20131029170), and the Tsinghua University Initiative Scientific
Research Program.
NR 159
TC 11
Z9 11
U1 2
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2016
VL 820
IS 2
AR 89
DI 10.3847/0004-637X/820/2/89
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI8HE
UT WOS:000373741300008
ER
PT J
AU Fujii, Y
Spiegel, DS
Mroczkowski, T
Nordhaus, J
Zimmerman, NT
Parsons, AR
Mirbabayi, M
Madhusudhan, N
AF Fujii, Yuka
Spiegel, David S.
Mroczkowski, Tony
Nordhaus, Jason
Zimmerman, Neil T.
Parsons, Aaron R.
Mirbabayi, Mehrdad
Madhusudhan, Nikku
TI RADIO EMISSION FROM RED-GIANT HOT JUPITERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planets and satellites: individual (Jupiter); radio
continuum: planetary systems; stars: AGB and post-AGB; stars: evolution;
Sun: evolution
ID PLANETARY MAGNETIC-FIELDS; STELLAR WIND CONDITIONS; MASS-LOSS RATES;
EXTRASOLAR PLANETS; CONTINUUM EMISSION; BROWN DWARFS; WHITE-DWARFS;
POWER SPECTRUM; ALPHA-ORIONIS; SCALING LAW
AB When planet-hosting stars evolve off the main sequence and go through the red-giant branch, the stars become orders of magnitudes more luminous and, at the same time, lose mass at much higher rates than their main-sequence counterparts. Accordingly, if planetary companions exist around these stars at orbital distances of a few au, they will be heated up to the level of canonical hot Jupiters and also be subjected to a dense stellar wind. Given that magnetized planets interacting with stellar winds emit radio waves, such "Red-Giant Hot Jupiters" (RGHJs) may also be candidate radio emitters. We estimate the spectral auroral radio intensity of RGHJs based on the empirical relation with the stellar wind as well as a proposed scaling for planetary magnetic fields. RGHJs might be intrinsically as bright as or brighter than canonical hot Jupiters and about 100 times brighter than equivalent objects around main-sequence stars. We examine the capabilities of low-frequency radio observatories to detect this emission and find that the signal from an RGHJ may be detectable at distances up to a few hundred parsecs with the Square Kilometer Array.
C1 [Fujii, Yuka] Tokyo Inst Technol, Earth Life Sci Inst, Tokyo 1528550, Japan.
[Fujii, Yuka] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Spiegel, David S.] Stitch Fix, Analyt & Algorithms, San Francisco, CA 94103 USA.
[Spiegel, David S.] Sum Labs, Res & Dev, New York, NY 10001 USA.
[Spiegel, David S.; Mirbabayi, Mehrdad] Inst Adv Study, Dept Astrophys, Olden Lane, Princeton, NJ 08540 USA.
[Mroczkowski, Tony] Naval Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA.
[Nordhaus, Jason] Rochester Inst Technol, Natl Tech Inst Deaf, Dept Sci & Math, Rochester, NY 14623 USA.
[Nordhaus, Jason] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA.
[Zimmerman, Neil T.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Parsons, Aaron R.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
[Madhusudhan, Nikku] Univ Cambridge, Dept Astron, Cambridge CB2 1TN, England.
RP Fujii, Y (reprint author), Tokyo Inst Technol, Earth Life Sci Inst, Tokyo 1528550, Japan.; Fujii, Y (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM yuka.fujii@elsi.jp
OI Zimmerman, Neil/0000-0001-5484-1516; Mroczkowski,
Tony/0000-0003-3816-5372
FU Japan Society for the Promotion of Science [25887024]; AMIAS group; NASA
[AR-12146.04-A]; NSF [AST-1102738, 1352519, 1440343]; National Research
Council Research Associateship Award at the Naval Research Laboratory
(NRL); NASA Postdoctoral Program at NASA Goddard Institute for Space
Studies
FX Y.F. is supported from the Grant-in-Aid No. 25887024 by the Japan
Society for the Promotion of Science and from an appointment to the NASA
Postdoctoral Program at NASA Goddard Institute for Space Studies,
administered by Oak Ridge Affiliated Universities. D.S.S. gratefully
acknowledges support from a fellowship from the AMIAS group. J.N.
acknowledges support from NASA grant HST AR-12146.04-A and NSF grant
AST-1102738. We thank David Hogg for encouraging us to pursue
calculations of exoplanetary radio emission. We thank Greg Novak for
helpful conversations. We thank Jake VanderPlas for developing the
XKCD-style plotting package for matplotlib, and acknowledge its use.
A.P. is grateful for support from NSF grants 1352519 and 1440343. Y.F.
greatly acknowledges insightful and helpful discussions with Tomoki
Kimura and Hiroki Harakawa. The portion of this research for which T.M.
is responsible was performed under a National Research Council Research
Associateship Award at the Naval Research Laboratory (NRL). Basic
research in radio astronomy at NRL is supported by 6.1 Base funding.
NR 94
TC 1
Z9 1
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2016
VL 820
IS 2
AR 122
DI 10.3847/0004-637X/820/2/122
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI8HE
UT WOS:000373741300041
ER
PT J
AU Gehrels, N
Cannizzo, JK
Kanner, J
Kasliwal, MM
Nissanke, S
Singer, LP
AF Gehrels, Neil
Cannizzo, John K.
Kanner, Jonah
Kasliwal, Mansi M.
Nissanke, Samaya
Singer, Leo P.
TI GALAXY STRATEGY FOR LIGO-VIRGO GRAVITATIONAL WAVE COUNTERPART SEARCHES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: statistics; gamma-ray burst: general; gravitational waves;
X-rays: general
ID NEUTRON-STAR MERGERS; GAMMA-RAY BURSTS; COMPACT OBJECT MERGERS;
RADIOACTIVELY POWERED TRANSIENTS; LUMINOSITY FUNCTION; ELECTROMAGNETIC
COUNTERPARTS; REDSHIFT SURVEY; BINARY MERGERS; MASS EJECTION; JET BREAKS
AB In this work we continue a line of inquiry begun in Kanner et al. which detailed a strategy for utilizing telescopes with narrow fields of view, such as the Swift X-ray Telescope (XRT), to localize gravitational wave (GW) triggers from LIGO/Virgo. If one considers the brightest galaxies that produce similar to 50% of the light, then the number of galaxies inside typical GW error boxes will be several tens. We have found that this result applies both in the early years of Advanced LIGO when the range was small and the error boxes were large, and will apply in the later years when the error boxes will be small and the range will be large. This strategy has the beneficial property of reducing the number of telescope pointings by a factor of 10-100 compared with tiling the entire error box. Additional galaxy count reduction will come from a GW rapid distance estimate which will restrict the radial slice in search volume. Combining the bright galaxy strategy with a convolution based on anticipated GW localizations, we find that the searches can be restricted to about 18 +/- 5 galaxies for 2015, about 23 +/- 4 for 2017, and about 11 +/- 2 for 2020. This assumes a distance localization at the putative neutron star-neutron star merger range mu for each target year, and these totals are integrated out to the range. Integrating out to the horizon would roughly double the totals. For localizations with r << mu the totals would decrease. The galaxy strategy we present in this work will enable numerous sensitive optical and XRTs with small fields of view to participate meaningfully in searches wherein the prospects for rapidly fading afterglow place a premium on a fast response time.
C1 [Gehrels, Neil; Singer, Leo P.] NASA, Goddard Space Flight Ctr, Mail Code 661, Greenbelt, MD 20771 USA.
[Cannizzo, John K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Cannizzo, John K.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Cannizzo, John K.] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Kanner, Jonah] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Kasliwal, Mansi M.] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA.
[Nissanke, Samaya] Radboud Univ Nijmegen, Inst Math Astrophys & Particle Phys, Heyendaalseweg 135, NL-6525 AJ Nijmegen, Netherlands.
RP Gehrels, N (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 661, Greenbelt, MD 20771 USA.
OI Singer, Leo/0000-0001-9898-5597; Kanner, Jonah/0000-0001-8115-0577
FU Carnegie-Princeton Fellowship; NSF [1066293]; Radboud University
Excellence Initiative
FX M.M.K. acknowledges generous support from the Carnegie-Princeton
Fellowship. S.N. and L.P.S. thank the Aspen Center for Physics and the
NSF Grant #1066293 for hospitality during the editing of this paper.
S.N. acknowledges generous support from the Radboud University
Excellence Initiative. We thank internal LIGO reviewer Ilya Mandel for
excellent feedback on all aspects of the paper.
NR 94
TC 10
Z9 10
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2016
VL 820
IS 2
AR 136
DI 10.3847/0004-637X/820/2/136
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI8HE
UT WOS:000373741300055
ER
PT J
AU Jensen-Clem, R
Millar-Blanchaer, M
Mawet, D
Graham, JR
Wallace, JK
Macintosh, B
Hinkley, S
Wiktorowicz, SJ
Perrin, MD
Marley, MS
Fitzgerald, MP
Oppenheimer, R
Ammons, SM
Rantakyr, FT
Marchis, F
AF Jensen-Clem, Rebecca
Millar-Blanchaer, Max
Mawet, Dimitri
Graham, James R.
Wallace, J. Kent
Macintosh, Bruce
Hinkley, Sasha
Wiktorowicz, Sloane J.
Perrin, Marshall D.
Marley, Mark S.
Fitzgerald, Michael P.
Oppenheimer, Rebecca
Ammons, S. Mark
Rantakyr, Fredrik T.
Marchis, Franck
TI POINT SOURCE POLARIMETRY WITH THE GEMINI PLANET IMAGER: SENSITIVITY
CHARACTERIZATION WITH T5.5 DWARF COMPANION HD 19467 B
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; stars: individual (HD 19467); techniques: high angular
resolution; techniques: polarimetric
ID BROWN DWARFS; HR 8799; LINEAR-POLARIZATION; T DWARFS; TRANSITION;
SPECTROSCOPY; VARIABILITY; ATMOSPHERES; DISCOVERY; WEATHER
AB Detecting polarized light from self-luminous exoplanets has the potential to provide key information about rotation, surface gravity, cloud grain size, and cloud coverage. While field brown dwarfs with detected polarized emission are common, no exoplanet or substellar companion has yet been detected in polarized light. With the advent of high contrast imaging spectro-polarimeters such as GPI and SPHERE, such a detection may now be possible with careful treatment of instrumental polarization. In this paper, we present 28 minutes of H-band GPI polarimetric observations of the benchmark T5.5 companion HD 19467 B. We detect no polarization signal from the target, and place an upper limit on the degree of linear polarization of p(CL99.73%) <= 2.4%. We discuss our results in the context of T dwarf cloud models and photometric variability.
C1 [Jensen-Clem, Rebecca; Mawet, Dimitri] CALTECH, Dept Astrophys, 1200 E Calif Blvd, Pasadena, CA 91101 USA.
[Millar-Blanchaer, Max] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
[Millar-Blanchaer, Max] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Graham, James R.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
[Wallace, J. Kent] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Macintosh, Bruce] Stanford Univ, Dept Phys, Palo Alto, CA 94304 USA.
[Macintosh, Bruce] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Palo Alto, CA 94304 USA.
[Hinkley, Sasha] Univ Exeter, Dept Phys, Stocker Rd, Exeter EX4 4QL, Devon, England.
[Wiktorowicz, Sloane J.] Univ Calif Santa Cruz, Dept Astron, 1156 High St, Santa Cruz, CA 95064 USA.
[Perrin, Marshall D.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Marley, Mark S.] NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.
[Fitzgerald, Michael P.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Oppenheimer, Rebecca] Amer Museum Nat Hist, New York, NY 10024 USA.
[Ammons, S. Mark] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA.
[Rantakyr, Fredrik T.] Gemini Observ, Casilla 603, La Serena, Chile.
[Marchis, Franck] Carl Sagan Ctr, SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
RP Jensen-Clem, R (reprint author), CALTECH, Dept Astrophys, 1200 E Calif Blvd, Pasadena, CA 91101 USA.
OI Marley, Mark/0000-0002-5251-2943; Perrin, Marshall/0000-0002-3191-8151;
Fitzgerald, Michael/0000-0002-0176-8973
FU National Science Foundation Graduate Research Fellowship [DGE-1144469];
NASA through the Sagan Fellowship Program; U.S. Department of Energy
[DE-AC52-07NA27344]
FX This material is based upon work supported by the National Science
Foundation Graduate Research Fellowship under grant No. DGE-1144469.
This work was performed in part under contract with the California
Institute of Technology (Caltech) funded by NASA through the Sagan
Fellowship Program executed by the NASA Exoplanet Science Institute, and
under the auspices of the U.S. Department of Energy by Lawrence
Livermore National Laboratory under Contract DE-AC52-07NA27344.
NR 49
TC 4
Z9 4
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2016
VL 820
IS 2
AR 111
DI 10.3847/0004-637X/820/2/111
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI8HE
UT WOS:000373741300030
ER
PT J
AU Jones, SI
Davila, JM
Uritsky, V
AF Jones, Shaela I.
Davila, Joseph M.
Uritsky, Vadim
TI OPTIMIZING GLOBAL CORONAL MAGNETIC FIELD MODELS USING IMAGE-BASED
CONSTRAINTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: miscellaneous; Sun: corona; Sun: magnetic fields
ID FORCE-FREE FIELD; SOLAR CORONA; WIND; EXTRAPOLATION; PERSPECTIVES;
EVOLUTION; STEREO; LOOPS; CYCLE
AB The coronal magnetic field directly or indirectly affects a majority of the phenomena studied in the heliosphere. It provides energy for coronal heating, controls the release of coronal mass ejections, and drives heliospheric and magnetospheric activity, yet the coronal magnetic field itself has proven difficult to measure. This difficulty has prompted a decades-long effort to develop accurate, timely, models of the field-an effort that continues today. We have developed a method for improving global coronal magnetic field models by incorporating the type of morphological constraints that could be derived from coronal images. Here we report promising initial tests of this approach on two theoretical problems, and discuss opportunities for application.
C1 [Jones, Shaela I.; Davila, Joseph M.; Uritsky, Vadim] NASA, Goddard Space Flight Ctr, Code 670, Greenbelt, MD 20771 USA.
[Jones, Shaela I.; Uritsky, Vadim] Catholic Univ Amer, Washington, DC 20064 USA.
RP Jones, SI (reprint author), NASA, Goddard Space Flight Ctr, Code 670, Greenbelt, MD 20771 USA.
EM shaela.i.jonesmecholsky@nasa.gov
NR 42
TC 0
Z9 0
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2016
VL 820
IS 2
AR 113
DI 10.3847/0004-637X/820/2/113
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI8HE
UT WOS:000373741300032
ER
PT J
AU Kipping, DM
Torres, G
Henze, C
Teachey, A
Isaacson, H
Petigura, E
Marcy, GW
Buchhave, LA
Chen, J
Bryson, ST
Sandford, E
AF Kipping, D. M.
Torres, G.
Henze, C.
Teachey, A.
Isaacson, H.
Petigura, E.
Marcy, G. W.
Buchhave, L. A.
Chen, J.
Bryson, S. T.
Sandford, E.
TI A TRANSITING JUPITER ANALOG
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planets and satellites: detection; stars: individual
(KIC-3239945, KOI-490, Kepler-167); techniques: photometric
ID MULTI-PLANET SYSTEMS; KEPLER INPUT CATALOG; GIANT PLANETS; FALSE
POSITIVES; HABITABLE ZONE; SNOW-LINE; EXTRASOLAR PLANETS; BLEND
SCENARIOS; HOST STARS; EXOPLANET
AB Decadal-long radial velocity surveys have recently started to discover analogs to the most influential planet of our solar system, Jupiter. Detecting and characterizing these worlds is expected to shape our understanding of our uniqueness in the cosmos. Despite the great successes of recent transit surveys, Jupiter analogs represent a terra incognita, owing to the strong intrinsic bias of this method against long orbital periods. We here report on the first validated transiting Jupiter analog, Kepler-167e (KOI-490.02), discovered using Kepler archival photometry orbiting the K4-dwarf KIC-3239945. With a radius of (0.91 +/- 0.02) R-J, a low orbital eccentricity (0.06(-0.04)(+0.10)), and an equilibrium temperature of(131 +/- 3) K, Kepler-167e bears many of the basic hallmarks of Jupiter. Kepler-167e is accompanied by three Super-Earths on compact orbits, which we also validate, leaving a large cavity of transiting worlds around the habitable-zone. With two transits and continuous photometric coverage, we are able to uniquely and precisely measure the orbital period of this post snow-line planet (1071.2323 +/- 0.0006d), paving the way for follow-up of this K = 11.8 mag target.
C1 [Kipping, D. M.; Teachey, A.; Chen, J.; Sandford, E.] Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA.
[Torres, G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Henze, C.; Bryson, S. T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Isaacson, H.; Petigura, E.; Marcy, G. W.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
RP Kipping, DM (reprint author), Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA.
EM dkipping@astro.columbia.edu
OI Isaacson, Howard/0000-0002-0531-1073
FU NASA [NNX14AB83G, NNX15AF09G]
FX This work made use of the Michael Dodds Computing Facility and the
Pleiades supercomputer at NASA Ames. G.T. acknowledges partial support
for this work from NASA grant NNX14AB83G (Kepler Participating Scientist
Program). D.M.K. acknowledges partial support from NASA grant NNX15AF09G
(NASA ADAP Program). This research has made use of the Exoplanet Orbit
Database and the Exoplanet Data Explorer at exoplanets.org, and the
corner.py code by Dan Foreman-Mackey at github.com/dfm/corner.py. We
offer our thanks and praise to the extraordinary scientists, engineers,
and individuals who have made the Kepler mission possible. Finally, the
authors wish to extend special thanks to those of Hawaiian ancestry on
whose sacred mountain of Mauna Kea we are privileged to be guests.
Without their generous hospitality, the Keck observations presented
herein would not have been possible.
NR 74
TC 6
Z9 6
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2016
VL 820
IS 2
AR 112
DI 10.3847/0004-637X/820/2/112
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI8HE
UT WOS:000373741300031
ER
PT J
AU Kowalski, AF
Mathioudakis, M
Hawley, SL
Wisniewski, JP
Dhillon, VS
Marsh, TR
Hilton, EJ
Brown, BP
AF Kowalski, Adam F.
Mathioudakis, Mihalis
Hawley, Suzanne L.
Wisniewski, John P.
Dhillon, Vik S.
Marsh, Tom R.
Hilton, Eric J.
Brown, Benjamin P.
TI M DWARF FLARE CONTINUUM VARIATIONS ON ONE-SECOND TIMESCALES: CALIBRATING
AND MODELING OF ULTRACAM FLARE COLOR INDICES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: flare; stars: low-mass
ID STAR YZ CMI; RADIATIVE HYDRODYNAMIC MODELS; WHITE-LIGHT FLARES; X-RAY;
SOLAR-FLARE; STELLAR FLARES; OPTICAL-SPECTRA; AD LEONIS; MULTIWAVELENGTH
OBSERVATIONS; ELECTRON ACCELERATION
AB We present a large data. set of high-cadence dMe flare light curves obtained with custom continuum filters on the triple-beam, high-speed camera system ULTRACAM. The measurements provide constraints for models of the near-ultraviolet (NUV) and optical continuum spectral evolution on timescales of approximate to 1 s. We provide a robust interpretation of the flare emission in the ULTRACAM filters using simultaneously obtained low-resolution spectra during two moderate-sized flares in the dM4.5e star YZ CMi. By avoiding the spectral complexity within the broadband Johnson filters, the ULTRACAM filters are shown to characterize bona. fide continuum emission in the NUV, blue, and red wavelength regimes. The NUV/blue flux ratio in flares is equivalent to a Balmer jump ratio, and the blue/red flux ratio provides an estimate for the color temperature of the optical continuum emission. We present a new "color-color" relationship for these continuum flux ratios at the peaks of the flares. Using the RADYN and RH codes, we interpret the ULTRACAM filter emission using the dominant emission processes from a radiative-hydrodynamic flare model with a high nonthermal electron beam flux, which explains a hot, T approximate to 10(4) K, color temperature at blue-to-red optical wavelengths and a small Balmer jump ratio as. observed in moderate-sized and large flares alike. We also discuss the high time resolution, high signal-to-noise continuum color variations observed in YZ CMi during a giant flare, which increased the NUV flux from this star by over a factor of 100.
C1 [Kowalski, Adam F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Kowalski, Adam F.] NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
[Mathioudakis, Mihalis] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Hawley, Suzanne L.; Hilton, Eric J.] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
[Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, 440 Brooks St, Norman, OK 73019 USA.
[Dhillon, Vik S.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England.
[Dhillon, Vik S.] Inst Astrofis Canarias, San Cristobal la Laguna 38205, Santa Cruz De T, Spain.
[Marsh, Tom R.] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England.
[Brown, Benjamin P.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Brown, Benjamin P.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
RP Kowalski, AF (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.; Kowalski, AF (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
EM adam.f.kowalski@nasa.gov
FU NSF [AST08-07205]; NASA Postdoctoral Program at the Goddard Space Flight
Center; UMBC Goddard Planetary Heliophysics Institute (GPHI) [132];
European Community [606862]; STFC [ST/L00073]
FX A.F.K. acknowledges the support from NSF grant AST08-07205, the NASA
Postdoctoral Program at the Goddard Space Flight Center, administered by
Oak Ridge Associated Universities through a contract with NASA, and from
UMBC Goddard Planetary Heliophysics Institute (GPHI) Task 132. M. M.
acknowledges support from the European Community's Seventh Framework
Programme (FP7/2007-2013) under grant agreement No. 606862 (F-CHROMA).
T.R.M. acknowledges support from the STFC, ST/L00073. A.F.K.
acknowledges Dr. J. Holtzman for providing the U-band data from the NMSU
1 m telescope at the APO, Dr. S.J. Schmidt for supporting observations
with ARCSAT at the APO, Dr. C. Copperwheat and Dr. S. Littlefair for
assistance with ULTRACAM observations at the NTT, Dr. J. Allred for
helpful discussions about flare modeling and for assistance with the
RADYN and RH codes, Dr. M. Carlsson for helpful assistance with the
RADYN code, Dr. H. Uitenbroek for helpful assistance with the RH code,
Dr. P. Yoachim for discussions about spectra obtained with a wide slit,
Dr. R. Ryans for installing the ULTRACAM data reduction pipeline, and
Dr. L. Kleint for discussions about the interpretation of excess flare
emission.
NR 76
TC 3
Z9 3
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2016
VL 820
IS 2
AR 95
DI 10.3847/0004-637X/820/2/95
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI8HE
UT WOS:000373741300014
ER
PT J
AU Liu, N
Nittler, LR
Alexander, CMO
Wang, JH
Pignatari, M
Jose, J
Nguyen, A
AF Liu, Nan
Nittler, Larry R.
Alexander, Conel M. O'D.
Wang, Jianhua
Pignatari, Marco
Jose, Jordi
Ann Nguyen
TI STELLAR ORIGINS OF EXTREMELY C-13- AND N-15-ENRICHED PRESOLAR SIC
GRAINS: NOVAE OR SUPERNOVAE?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; meteorites, meteors, meteoroids; novae,
cataclysmic variables; nuclear, reactions, nucleosynthesis, abundances;
supernovae: general
ID SILICON-CARBIDE GRAINS; GIANT BRANCH STARS; ISOTOPIC COMPOSITIONS;
MASSIVE STARS; CARBON STARS; MURCHISON METEORITE; GALACTIC EVOLUTION;
CLASSICAL NOVAE; SOLAR-SYSTEM; SI3N4 GRAINS
AB Extreme excesses of C-13 (C-12/C-13 < 10) and N-15 (N-14/N-15 < 20) in rare presolar SiC grains have been considered diagnostic of an origin in classical novae, though an origin in core collapse supernovae (CCSNe) has also been proposed. We report C, N, and Si isotope data for 14 submicron-to micron-sized C-13-and N-15-enriched presolar SiC grains (C-12/C-13 < 16 and N-14/N-15 < similar to 100) from Murchison, and their correlated Mg-Al, S, and Ca-Ti isotope data when available. These grains are enriched in C-13 and N-15, but with quite diverse Si isotopic signatures. Four grains with Si-29,Si-30 excesses similar to those of type C SiC grains likely came from CCSNe, which experienced explosive H burning occurred during explosions. The independent coexistence of proton-and neutron-capture isotopic signatures in these grains strongly supports heterogeneous H ingestion into the He shell in pre-supernovae. Two of the seven putative nova grains with Si-30 excesses and Si-29 depletions show lower-than-solar S-34/S-32 ratios that cannot be explained by classical nova nucleosynthetic models. We discuss these signatures within the CCSN scenario. For the remaining five putative nova grains, both nova and supernova origins are viable because explosive H burning in the two stellar sites could result in quite similar proton-capture isotopic signatures. Three of the grains are sub-type AB grains that are also 13C enriched, but have a range of higher 14N/15N. We found that N-15-enriched AB grains (similar to 50 < 14N/15N < similar to 100) have distinctive isotopic signatures compared to putative nova grains, such as higher 14N/15N, lower Al-26/Al-27, and lack of 30Si excess, indicating weaker proton-capture nucleosynthetic environments.
C1 [Liu, Nan; Nittler, Larry R.; Alexander, Conel M. O'D.; Wang, Jianhua] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
[Pignatari, Marco] Univ Hull, Dept Math & Phys, EA Milne Ctr Astrophys, Kingston Upon Hull HU6 7RX, N Humberside, England.
[Pignatari, Marco] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary.
[Jose, Jordi] Univ Politecn Cataluna, EUETIB, Dept Fis, E-08036 Barcelona, Spain.
[Jose, Jordi] Inst Estudis Espacials Catalunya, E-08034 Barcelona, Spain.
[Ann Nguyen] NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA.
[Ann Nguyen] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Liu, N (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
EM nliu@carnegiescience.edu
RI Wang, Jianhua/D-6500-2011;
OI Wang, Jianhua/0000-0002-7671-2413; Alexander, Conel/0000-0002-8558-1427
FU NASA's Cosmochemistry program [NNX10AI63G]; NSF [PHY 09-22648,
PHY-1430152]; Hungarian Academy of Sciences (Hungary); SNF
(Switzerland); STFC's DiRAC High Performance Computing Facilities;
Spanish MINECO grant [AYA2013-42762-P, AYA2014-59084-P]; Generalitat de
Catalunya grant [SGR0038/2014]
FX We thank Alexander Heger for providing CCSN nucleosynthetic model
calculations. This work was supported by NASA's Cosmochemistry program
(grant NNX10AI63G to LRN). M.P. acknowledges significant support to
NuGrid from NSF grants PHY 09-22648 (Joint Institute for Nuclear
Astrophysics, JINA), NSF grant PHY-1430152 (JINA Center for the
Evolution of the Elements), and EU MIRGCT-2006-046520. M.P. acknowledges
the support from the "Lendulet-2014" Program of the Hungarian Academy of
Sciences (Hungary) and from SNF (Switzerland). M.P. also acknowledges
PRACE, through its Distributed Extreme Computing Initiative, for
resource allocations on Sisu (CSC, Finland), Archer (EPCC, UK), and
Beskow (KTH, Sweden). We acknowledge the support of STFC's DiRAC High
Performance Computing Facilities; DiRAC is part of the National
E-infrastructure. Ongoing resource allocations on the University of
Hull's High Performance Computing Facility-viper-are gratefully
acknowledged. J.J. acknowledges the Spanish MINECO grants
AYA2013-42762-P and AYA2014-59084-P, and the Generalitat de Catalunya
grant SGR0038/2014 for support.
NR 82
TC 0
Z9 0
U1 4
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2016
VL 820
IS 2
AR 140
DI 10.3847/0004-637X/820/2/140
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI8HE
UT WOS:000373741300059
ER
PT J
AU Ma, YK
Ng, CY
Bucciantini, N
Slane, PO
Gaensler, BM
Temim, T
AF Ma, Y. K.
Ng, C-Y.
Bucciantini, N.
Slane, P. O.
Gaensler, B. M.
Temim, T.
TI RADIO POLARIZATION OBSERVATIONS OF THE SNAIL: A CRUSHED PULSAR WIND
NEBULA IN G327.1-1.1 WITH A HIGHLY ORDERED MAGNETIC FIELD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (G327.1-1.1); ISM: supernova remnants; radio
continuum: ISM
ID SUPERNOVA REMNANT G327.1-1.1; X-RAY-EMISSION; IGR J11014-6103;
EVOLUTION; CHANDRA; CONSTRAINTS; MODEL; JET
AB Pulsar wind nebulae (PWNe) are suggested to be acceleration sites of cosmic rays in the Galaxy. While the magnetic field plays an important role in the acceleration process, previous observations of magnetic field configurations of PWNe are rare, particularly for evolved systems. We present a radio polarization study of the "Snail" PWN inside the supernova remnant G327.1-1.1 using the Australia Telescope Compact Array. This PWN is believed to have been recently crushed by the supernova (SN) reverse shock. The radio morphology is composed of a main circular body with a finger-like protrusion. We detected a strong linear polarization signal from the emission, which reflects a highly ordered magnetic field in the PWN and is in contrast to the turbulent environment with a tangled magnetic field generally expected from hydrodynamical simulations. This could suggest that the characteristic turbulence scale is larger than the radio beam size. We built a toy model to explore this possibility, and found that a simulated PWN with a turbulence scale of about one-eighth to one-sixth of the nebula radius and a pulsar wind filling factor of 50%-75% provides the best match to observations. This implies substantial mixing between the SN ejecta and pulsar wind material in this system.
C1 [Ma, Y. K.; Ng, C-Y.] Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China.
[Bucciantini, N.] INAF Osservatorio Astrofis Arcetri, Lgo E Fermi 5, I-50125 Florence, Italy.
[Bucciantini, N.] INFN Sez Firenze, Via G Sansone 1, I-50019 Florence, Italy.
[Slane, P. O.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Temim, T.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
[Temim, T.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
RP Ng, CY (reprint author), Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China.
EM ncy@bohr.physics.hku.hk
OI /0000-0002-5847-2612; Gaensler, Bryan/0000-0002-3382-9558; Temim,
Tea/0000-0001-7380-3144
FU Commonwealth of Australia; Australian Research Council; Science
Foundation for Physics within the University of Sydney; ECS grant of
Hong Kong Government [HKU 709713P]; NASA [NAS8-03060]
FX The authors thank J. Lim for fruitful discussions. We also thank an
anonymous referee for helpful comments and suggestions which improved
the paper. The Australia Telescope Compact Array is part of the
Australia Telescope National Facility which is funded by the
Commonwealth of Australia for operation as a National Facility managed
by CSIRO. MOST is operated by The University of Sydney with support from
the Australian Research Council and the Science Foundation for Physics
within the University of Sydney. This work is supported by ECS grant of
Hong Kong Government under HKU 709713P. P.O.S. acknowledges partial
support from NASA Contract NAS8-03060.
NR 40
TC 1
Z9 1
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2016
VL 820
IS 2
AR 100
DI 10.3847/0004-637X/820/2/100
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI8HE
UT WOS:000373741300019
ER
PT J
AU Mahjoub, A
Poston, MJ
Hand, KP
Brown, ME
Hodyss, R
Blacksberg, J
Eiler, JM
Carlson, RW
Ehlmann, BL
Choukroun, M
AF Mahjoub, Ahmed
Poston, Michael J.
Hand, Kevin P.
Brown, Michael E.
Hodyss, Robert
Blacksberg, Jordana
Eiler, John M.
Carlson, Robert W.
Ehlmann, Bethany L.
Choukroun, Mathieu
TI ELECTRON IRRADIATION AND THERMAL PROCESSING OF MIXED-ICES OF POTENTIAL
RELEVANCE TO JUPITER TROJAN ASTEROIDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; Kuiper Belt: general; methods: laboratory: molecular;
molecular processes; techniques: spectroscopic
ID OUTER SOLAR-SYSTEM; INFRARED-SPECTROSCOPY; OPTICAL-CONSTANTS; FROZEN
METHANOL; ION IRRADIATION; OCN-FORMATION; DENSE CLOUDS; IR-SPECTRA;
ANALOGS; AMMONIA
AB In this work we explore the chemistry that occurs during the irradiation of ice mixtures on planetary surfaces, with the goal of linking the presence of specific chemical compounds to their formation locations in the solar system and subsequent processing by later migration inward. We focus on the outer solar system and the chemical differences for ice mixtures inside and outside the stability line for H2S. We perform a set of experiments to explore the hypothesis advanced by Wong & Brown that links the color bimodality in Jupiter's Trojans to the presence of H2S in the surface of their precursors. Non-thermal (10 keV electron irradiation) and thermally driven chemistry of CH3OH-NH3-H2O ("without H2S") and H2S-CH3OH-NH3-H2O ("with H2S") ices were examined. Mid-IR analyses of ice and mass spectrometry monitoring of the volatiles released during heating show a rich chemistry in both of the ice mixtures. The "with H2S" mixture experiment shows a rapid consumption of H2S molecules and production of OCS molecules after a few hours of irradiation. The heating of the irradiated "with H2S" mixture to temperatures above 120 K leads to the appearance of new infrared bands that we provisionally assign to SO2 and CS. We show that radiolysis products are stable under the temperature and irradiation conditions of Jupiter Trojan asteroids. This makes them suitable target molecules for potential future missions as well as telescope observations with a high signal-to-noise ratio. We also suggest the consideration of sulfur chemistry in the theoretical modeling aimed at understanding the chemical composition of Trojans and KOBs.
C1 [Mahjoub, Ahmed; Poston, Michael J.; Hand, Kevin P.; Hodyss, Robert; Blacksberg, Jordana; Carlson, Robert W.; Ehlmann, Bethany L.; Choukroun, Mathieu] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Mahjoub, Ahmed; Poston, Michael J.; Brown, Michael E.; Eiler, John M.; Ehlmann, Bethany L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Mahjoub, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Mahjoub, A (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM Mahjoub.Ahmed@jpl.nasa.gov
RI Choukroun, Mathieu/F-3146-2017;
OI Choukroun, Mathieu/0000-0001-7447-9139; Poston,
Michael/0000-0001-5113-1017
FU Keck Institute of Space Studies (KISS)
FX This work was conducted at the Jet Propulsion Laboratory, Caltech, under
a contract with the National Aeronautics and Space Administration (NASA)
and at the Caltech Division of Geological and Planetary Sciences. This
work was supported by the Keck Institute of Space Studies (KISS).
Government sponsorship is acknowledged.
NR 51
TC 2
Z9 2
U1 5
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2016
VL 820
IS 2
AR 141
DI 10.3847/0004-637X/820/2/141
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI8HE
UT WOS:000373741300060
ER
PT J
AU Sayers, J
Zemcov, M
Glenn, J
Golwala, SR
Maloney, PR
Siegel, SR
Wheeler, J
Bockstiegel, C
Brugger, S
Czakon, NG
Day, PK
Downes, TP
Duan, RP
Gao, JS
Hollister, MI
Lam, A
LeDuc, HG
Mazin, BA
McHugh, SG
Miller, DA
Mroczkowski, TK
Noroozian, O
Nguyen, HT
Radford, SJE
Schlaerth, JA
Vayonakis, A
Wilson, PR
Zmuidzinas, J
AF Sayers, Jack
Zemcov, Michael
Glenn, Jason
Golwala, Sunil R.
Maloney, Philip R.
Siegel, Seth R.
Wheeler, Jordan
Bockstiegel, Clint
Brugger, Spencer
Czakon, Nicole G.
Day, Peter K.
Downes, Thomas P.
Duan, Ran P.
Gao, Jiansong
Hollister, Matthew I.
Lam, Albert
LeDuc, Henry G.
Mazin, Benjamin A.
McHugh, Sean G.
Miller, David A.
Mroczkowski, Tony K.
Noroozian, Omid
Nguyen, Hien T.
Radford, Simon J. E.
Schlaerth, James A.
Vayonakis, Anastasios
Wilson, Philip R.
Zmuidzinas, Jonas
TI PECULIAR VELOCITY CONSTRAINTS FROM FIVE-BAND SZ EFFECT MEASUREMENTS
TOWARD RX J1347.5-1145 WITH MUSIC AND BOLOCAM FROM THE CSO
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual: (RX. J1347.5-1145); galaxies: clusters:
intracluster medium
ID SUNYAEV-ZELDOVICH SIGNAL; RELAXED GALAXY CLUSTERS; X-RAY-CLUSTER;
SCALING RELATIONS; MACS J0717.5+3745; PRESSURE PROFILES; SAMPLE; GHZ;
J1347-1145; COSMOLOGY
AB We present Sunyaev-Zel'dovich (SZ) effect measurements from wide-field images toward the galaxy cluster RX. J1347.5-1145 obtained from the Caltech Submillimeter Observatory with the Multiwavelength Submillimeter Inductance Camera at 147, 213, 281, and 337 GHz and with Bolocam at 140 GHz. As part of our analysis, we have used higher frequency data from Herschel-SPIRE and previously published lower frequency radio data to subtract the signal from the brightest dusty star-forming galaxies behind RX. J1347.5-1145 and from the AGN in RX. J1347.5-1145's BCG. Using these five-band SZ effect images, combined with X-ray spectroscopic measurements of the temperature of the intra-cluster medium (ICM) from Chandra, we constrain the ICM optical depth to be tau(e) = 7.33(-0.97)(+0.96) x 10(-3) and the ICM line of sight peculiar velocity to be v(pec) = 1040(-840)(+870) km s(-1). The errors for both quantities are limited by measurement noise rather than calibration uncertainties or astrophysical contamination, and significant improvements are possible with deeper observations. Our best-fit velocity is in good agreement with one previously published SZ effect analysis and in mild tension with the other, although some or all of that tension may be because that measurement samples a much smaller cluster volume. Furthermore, our best-fit optical depth implies a gas mass slightly larger than the Chandra-derived value, implying the cluster is elongated along the line of sight.
C1 [Sayers, Jack; Golwala, Sunil R.; Siegel, Seth R.; Hollister, Matthew I.; Lam, Albert; Miller, David A.; Radford, Simon J. E.; Schlaerth, James A.; Vayonakis, Anastasios; Zmuidzinas, Jonas] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Zemcov, Michael] Rochester Inst Technol, Rochester, NY 14623 USA.
[Glenn, Jason; Maloney, Philip R.; Wheeler, Jordan; Brugger, Spencer; Schlaerth, James A.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Bockstiegel, Clint; Mazin, Benjamin A.; McHugh, Sean G.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Czakon, Nicole G.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Day, Peter K.; LeDuc, Henry G.; Nguyen, Hien T.; Wilson, Philip R.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Downes, Thomas P.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA.
[Duan, Ran P.] Chinese Acad Sci, Natl Astron Observ, Beijing, Peoples R China.
[Gao, Jiansong] NIST, Boulder, CO 80305 USA.
[Mroczkowski, Tony K.] US Naval Res Lab, Washington, DC 20375 USA.
[Noroozian, Omid] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sayers, J (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
EM jack@caltech.edu
OI radford, simon/0000-0001-9113-1660; Mroczkowski,
Tony/0000-0003-3816-5372
FU Norris Foundation Fellowship; NASA Graduate Student Research Fellowship;
NASA Earth and Space Science Fellowship; Gordon and Betty Moore
Foundation; JPL internal funds; NSF; NASA
FX We thank the anonymous referee for his or her extensive suggestions to
improve this manuscript. We acknowledge the assistance of: the day crew
and Hilo staff of the Caltech Submillimeter Observatory, who provided
invaluable assistance during data-taking for this data set; Kathy
Deniston and Diana Bisel, who provided effective administrative support
at Caltech and in Hilo; J.S. was partially supported by a Norris
Foundation Fellowship; N.G.C. was partially supported by a NASA Graduate
Student Research Fellowship; S.R.S. was supported by a NASA Earth and
Space Science Fellowship; MUSIC was constructed and commissioned with
funding provided by the Gordon and Betty Moore Foundation, JPL internal
funds, and the NSF Advanced Technologies and Instrumentation (ATI) and
Astronomy and Astrophysics Grants (AAG) Programs. This work is based in
part on observations made with Herschel, a European Space Agency
Cornerstone Mission with a significant participation by NASA. Partial
support for this work was provided by NASA through an award issued by
JPL/Caltech. This research was performed while TM held a National
Research Council Research Associateship Award at the Naval Research
Laboratory.
NR 72
TC 3
Z9 3
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2016
VL 820
IS 2
AR 101
DI 10.3847/0004-637X/820/2/101
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DI8HE
UT WOS:000373741300020
ER
PT J
AU Lewis, JK
Bischof, JC
Braslavsky, I
Brockbank, KGM
Fahy, GM
Fuller, BJ
Rabin, Y
Tocchio, A
Woods, EJ
Wowk, BG
Acker, JP
Giwa, S
AF Lewis, Jedediah K.
Bischof, John C.
Braslavsky, Ido
Brockbank, Kelvin G. M.
Fahy, Gregory M.
Fuller, Barry J.
Rabin, Yoed
Tocchio, Alessandro
Woods, Erik J.
Wowk, Brian G.
Acker, Jason P.
Giwa, Sebastian
TI The Grand Challenges of Organ Banking: Proceedings from the first global
summit on complex tissue cryopreservation
SO CRYOBIOLOGY
LA English
DT Article
DE Organ banking; Organ preservation; Cryobanking; Organ transplantation;
Ice binding proteins; Antifreeze proteins; Cryoprotectant toxicity;
Chilling injury; Cryoprotectant screening; Thermo-mechanical stress;
Cryomacroscopy; Vitrification; Devitrification; Nanoparticle warming;
Ischemia; Freeze tolerance; Persufflation; Perfusion; Ischemic
preconditioning
ID INTRACELLULAR ICE FORMATION; ANTIFREEZE PROTEINS; UNITED-STATES;
VITRIFICATION; PRESERVATION; HIBERNATION; GROWTH; CELLS;
RECRYSTALLIZATION; TRANSPLANTATION
AB The first Organ Banking Summit was convened from Feb. 27 - March 1, 2015 in Palo Alto, CA, with events at Stanford University, NASA Research Park, and Lawrence Berkeley National Labs. Experts at the summit outlined the potential public health impact of organ banking, discussed the major remaining scientific challenges that need to be overcome in order to bank organs, and identified key opportunities to accelerate progress toward this goal. Many areas of public health could be revolutionized by the banking of organs and other complex tissues, including transplantation, oncofertility, tissue engineering, trauma medicine and emergency preparedness, basic biomedical research and drug discovery - and even space travel. Key remaining scientific sub-challenges were discussed including ice nucleation and growth, cryoprotectant and osmotic toxicities, chilling injury, thermo-mechanical stress, the need for rapid and uniform rewarming, and ischemia/reperfusion injury. A variety of opportunities to overcome these challenge areas were discussed, i.e. preconditioning for enhanced stress tolerance, nanoparticle rewarming, cyroprotectant screening strategies, and the use of cryoprotectant cocktails including ice binding agents.
C1 [Lewis, Jedediah K.; Tocchio, Alessandro; Giwa, Sebastian] NASA, Organ Preservat Alliance, Res Pk Bldg 20,S Akron Rd, Moffett Field, CA 94035 USA.
[Lewis, Jedediah K.; Tocchio, Alessandro] Stanford Univ, Palo Alto, CA 94304 USA.
[Bischof, John C.] Univ Minnesota, Dept Mech Engn, 111 Church St SE, Minneapolis, MN 55455 USA.
[Braslavsky, Ido] Hebrew Univ Jerusalem, Inst Biochem Food Sci & Nutr, Robert H Smith Fac Agr Food & Environm, IL-76100 Rehovot, Israel.
[Brockbank, Kelvin G. M.] Tissue Testing Technol LLC, N Charleston, SC USA.
[Brockbank, Kelvin G. M.] Clemson Univ, Dept Bioengn, Clemson, SC 29631 USA.
[Fahy, Gregory M.; Wowk, Brian G.] 21st Century Med Inc, Fontana, CA USA.
[Fuller, Barry J.] UCL Med Sch, Royal Free Hosp, Div Surg & Intervent Sci, Royal Free Hosp Campus, London, England.
[Rabin, Yoed] Carnegie Mellon Univ, Dept Mech Engn, Pittsburgh, PA 15213 USA.
[Woods, Erik J.; Acker, Jason P.] Soc Cryobiol, New York, NY USA.
[Woods, Erik J.] Cook Regentec, Indianapolis, IN USA.
[Acker, Jason P.] Canadian Blood Serv, Ctr Innovat, Edmonton, AB, Canada.
[Acker, Jason P.] Univ Alberta, Dept Lab Med & Pathol, Edmonton, AB, Canada.
[Giwa, Sebastian] Sylvatica Biotech Inc, Charleston, SC USA.
RP Giwa, S (reprint author), NASA, Organ Preservat Alliance, Res Pk Bldg 20,S Akron Rd, Moffett Field, CA 94035 USA.
EM sebastian.giwa@post.harvard.edu
FU Organ Preservation Alliance and Stanford Biomedical Engineering Society;
Thiel Foundation; Methuselah foundation; Organovo; Society for
Cryobiology; New Organ; Singularity University LABS at NASA Research
Park; Young Investigator Breakthroughs in Organ Banking Hackathon
FX This work was supported by: the Organ Preservation Alliance and Stanford
Biomedical Engineering Society which organized and hosted the overall
summit and sessions at Stanford respectively; the Thiel Foundation, the
Methuselah foundation and Organovo, which provided grants that made the
Summit possible; and the Society for Cryobiology, New Organ, and
Singularity University LABS at NASA Research Park, which supported the
Young Investigator Breakthroughs in Organ Banking Hackathon.
NR 70
TC 4
Z9 4
U1 12
U2 22
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0011-2240
EI 1090-2392
J9 CRYOBIOLOGY
JI Cryobiology
PD APR
PY 2016
VL 72
IS 2
BP 169
EP 182
DI 10.1016/j.cryobiol.2015.12.001
PG 14
WC Biology; Physiology
SC Life Sciences & Biomedicine - Other Topics; Physiology
GA DJ3BA
UT WOS:000374078600016
PM 26687388
ER
PT J
AU Schrader, CM
Cohen, BA
Donovan, JJ
Vicenzi, EP
AF Schrader, Christian M.
Cohen, Barbara A.
Donovan, John J.
Vicenzi, Edward P.
TI Ni/S/Cl systematics and the origin of impact-melt glasses in Martian
meteorite Elephant Moraine 79001
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID X-RAY SPECTROMETER; SHOCK METAMORPHISM; GUSEV CRATER; MERIDIANI-PLANUM;
SOIL COMPONENT; MARS; SHERGOTTITE; OLIVINE; A79001; ROCKS
AB Martian meteorite Elephant Moraine A79001 (EET 79001) has received considerable attention for the unusual composition of its shock melt glass, particularly its enrichment in sulfur relative to the host shergottite. It has been hypothesized that Martian regolith was incorporated into the melt or, conversely, that the S-enrichment stems from preferential melting of sulfide minerals in the host rock during shock. We present results from an electron microprobe study of EET 79001 including robust measurements of major and trace elements in the shock melt glass (S, Cl, Ni, Co, V, and Sc) and minerals in the host rock (Ni, Co, and V). We find that both S and major element abundances can be reconciled with previous hypotheses of regolith incorporation and/or excess sulfide melt. However, trace element characteristics of the shock melt glass, particularly Ni and Cl abundances relative to S, cannot be explained either by the incorporation of regolith or sulfide minerals. We therefore propose an alternative hypothesis whereby, prior to shock melting, portions of EET 79001 experienced acid-sulfate leaching of the mesostasis, possibly groundmass feldspar, and olivine, producing Al-sulfates that were later incorporated into the shock melt, which then quenched to glass. Such activity in the Martian near-surface is supported by observations from the Mars Exploration Rovers and laboratory experiments. Our preimpact alteration model, accompanied by the preferential survival of olivine and excess melting of feldspar during impact, explains the measured trace element abundances better than either the regolith incorporation or excess sulfide melting hypothesis does.
C1 [Schrader, Christian M.; Cohen, Barbara A.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Schrader, Christian M.] Bowdoin Coll, Dept Geol, Brunswick, ME 04011 USA.
[Donovan, John J.] Univ Oregon, Dept Chem, Eugene, OR 97403 USA.
[Vicenzi, Edward P.] Museum Conservat Inst, Smithsonian Inst, Suitland, MD 20746 USA.
RP Cohen, BA (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM barbara.a.cohen@nasa.gov
FU NASA Postdoctoral Program; Mars Fundamental Research Program grant
FX We thank the NASA Postdoctoral Program for funding salary and travel for
the first author, and the Antarctic Meteorite Working Group for
approving our sample request. Joel Hurowitz, Hap McSween, Paul Warren,
Erin Walton, and several anonymous reviewers provided helpful reviews
and editor Mike Zolensky encouraged us through several revisions. This
research was supported by a Mars Fundamental Research Program grant to
B. A. Cohen and used NASA's Astrophysics Data System (ADS).
NR 61
TC 0
Z9 0
U1 2
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD APR
PY 2016
VL 51
IS 4
BP 663
EP 680
DI 10.1111/maps.12612
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DJ2QT
UT WOS:000374050800003
ER
PT J
AU Harlan, S
Jenniskens, P
Zolensky, ME
Yin, QZ
Verosub, KL
Rowland, DJ
Sanborn, M
Huyskens, M
Creager, ER
Jull, AJT
AF Harlan, Scott
Jenniskens, Peter
Zolensky, Michael E.
Yin, Qing-Zhu
Verosub, Kenneth L.
Rowland, Douglas J.
Sanborn, Matthew
Huyskens, Magdalena
Creager, Emily R.
Jull, A. J. Timothy
CA Misfits Flat Meteorite Consortium
TI Meteorites found on Misfits Flat dry lake, Nevada
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID ORDINARY CHONDRITES; PETROGRAPHIC TYPE; CLASSIFICATION; EARTH;
ASTEROIDS; RECOVERY; ITOKAWA; ORIGIN; FALLS; FLUX
AB Meteorites have been found on the small Misfits Flat dry lakebed near Stagecoach, Nevada (119.382W, +39.348N). Since the first find on Sept. 22, 2013, a total of 58 stones of weathering stage W2/3 with a combined mass of 339g have been collected in 19 visits to the area. This small (3.3x3.6km) lakebed is now a newly designated dense collection area (DCA). Most meteorites were found in a small 350x180m area along the north shore and most are fragments of several broken individual stones. Three of these fragments were classified as an LL4/5 of shock stage S2, now named Misfits Flat 001, one of which (stone MF33) fell 8.1 +/- 1.3ka ago based on the C-14 terrestrial age, assuming it came from a 20-80cm diameter meteoroid. In addition, a small darkly crusted meteorite MF34, now named Misfits Flat 002, was found 820m WSW from the main mass. This meteorite is classified as an LL5 ordinary chondrite with shock stage S4/5. The meteorite is saturated in C-14 at 63dpmkg(-1), suggesting it originated from the center of a 0.5 m diameter meteoroid, or deep inside a similar to 1.0 m meteoroid, less than 300yr ago. Accounts exist of a fireball seen at 13:15 UT on March 2, 1895, that are consistent with the find location of Misfits Flat 002.
C1 [Harlan, Scott] Scott Harlan PE, 19518 Creekside Ct, Salinas, CA 93908 USA.
[Jenniskens, Peter] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Zolensky, Michael E.] NASA Johnson Space Ctr, Astromat Res & Explorat Sci, Houston, TX 77058 USA.
[Yin, Qing-Zhu; Verosub, Kenneth L.; Rowland, Douglas J.; Sanborn, Matthew; Huyskens, Magdalena] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA.
[Creager, Emily R.; Jull, A. J. Timothy] Univ Arizona, AMS Lab, Dept Phys, Tucson, AZ 85721 USA.
RP Jenniskens, P (reprint author), SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
EM petrus.m.jenniskens@nasa.gov
OI Rowland, Douglas/0000-0001-8059-6905; Sanborn,
Matthew/0000-0003-3218-1195
FU NASA [NNX14-AR92G, NNX14AM62G]; UC Office of the President (UC Lab Fees
Award) [12-LR-237921]
FX We thank Richard Medalen and Cheryl Harlan for their help in searching
and finding meteorites on Misfits Flat. We thank local resident Lester
Robertson for permission to search his property. S.H. thanks local
organizer Kees Welten for supporting his participation in the 2015
Meteoritical Society meeting and for helpful comments. We also thank
referee Beda Hofmann and an anonymous referee, as well as associate
editor Alex Ruzicka, for a careful reading of the paper and helpful
comments. This work was supported by NASA grant NNX14-AR92G (PJ) and
NNX14AM62G (QZY) and the UC Office of the President (UC Lab Fees Award
ID# 12-LR-237921 to QZY).
NR 45
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD APR
PY 2016
VL 51
IS 4
BP 757
EP 772
DI 10.1111/maps.12619
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DJ2QT
UT WOS:000374050800008
ER
PT J
AU Ito, M
Messenger, S
AF Ito, Motoo
Messenger, Scott
TI Rare earth element measurements and mapping of minerals in the Allende
CAI, 7R19-1, by NanoSIMS ion microprobe
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID CV3 CARBONACEOUS CHONDRITES; REFRACTORY INCLUSIONS; SOLAR-SYSTEM;
QUANTITATIVE-ANALYSIS; RICH INCLUSIONS; TRACE-ELEMENTS; PETROGENESIS;
NEBULA; SIMS; CONDENSATION
AB We have established analytical procedures for quantitative rare earth element (REE) measurements by NanoSIMS 50L ion microprobe with 2-10m spatial resolution. Measurements are performed by multidetection using energy filtering under several static magnetic field settings. Relative sensitivity factors and REE oxide/REE element secondary ion ratios that we determined for the NanoSIMS match values previously determined for other ion microprobes. REE measurements of 100ppm REE glass standards yielded reproducibility and accuracy of 0.5-2.5% and 5-15%, respectively. REE measurements of minerals of an Allende type-A CAI, 7R19-1, were performed using three different methods: spot analysis, line profile, and imaging. These data are in excellent agreement with previous REE measurements of this inclusion by IMS-3f ion microprobe. The higher spatial resolution NanoSIMS measurements provide additional insight into the formation process of this CAI and offer a promising new tool for analysis of fine-grained and complexly zoned materials.
C1 [Ito, Motoo; Messenger, Scott] NASA Johnson Space Ctr, Robert M Walker Lab Space Sci EISD ARES, EISD ARES, Mail Code XI3,2101 NASA Pkwy, Houston, TX 77058 USA.
[Ito, Motoo] JAMSTEC, Kochi Inst Core Sample Res, 200 Monobe Otsu, Nankoku, Kochi 7838502, Japan.
RP Ito, M (reprint author), NASA Johnson Space Ctr, Robert M Walker Lab Space Sci EISD ARES, EISD ARES, Mail Code XI3,2101 NASA Pkwy, Houston, TX 77058 USA.; Ito, M (reprint author), JAMSTEC, Kochi Inst Core Sample Res, 200 Monobe Otsu, Nankoku, Kochi 7838502, Japan.
EM motoo@jamstec.go.jp
FU NASA Cosmochemistry Program Grant
FX This research was inspired and made possible by the late Dr. Gordon
McKay. We thank Dr. Kevin Righter for his help in setting up the
laboratory facilities to produce the REE standards, and Drs. Anne
Peslier and Loan Le for their assistance in gathering the EPMA data.
This work was supported by a NASA Cosmochemistry Program Grant to S. M.
Constructive reviews by Drs. Andy Davis and Yunbin Guan greatly improved
the manuscript. We thank Dr. Christine Floss for editorial handling, and
useful comments and suggestions.
NR 44
TC 0
Z9 0
U1 3
U2 8
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD APR
PY 2016
VL 51
IS 4
BP 818
EP 832
DI 10.1111/maps.12623
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DJ2QT
UT WOS:000374050800012
ER
PT J
AU Sears, DWG
Sears, H
Ebel, DS
Wallace, S
Friedrich, JM
AF Sears, Derek W. G.
Sears, Hazel
Ebel, Denton S.
Wallace, Sean
Friedrich, Jon M.
TI X-ray computed tomography imaging: A not-so-nondestructive technique
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID THERMO-LUMINESCENCE; ORDINARY CHONDRITES; REHEATING HISTORY; METEORITES;
THERMOLUMINESCENCE; MICROTOMOGRAPHY; GEOSCIENCES; SAMPLES; SHOCK; CT
AB X-ray computed tomography has become a popular means for examining the interiors of meteorites and has been advocated for routine curation and for the examination of samples returned by missions. Here, we report the results of a blind test that indicate that CT imaging deposits a considerable radiation dose in a meteorite and seriously compromises its natural radiation record. Ten vials of the Bruderheim L6 chondrite were placed in CT imager and exposed to radiation levels typical for meteorite studies. Half were retained as controls. Their thermoluminescence (TL) properties were then measured in a blind test. Five of the samples had TL data unaltered from their original (similar to 10 cps) while five had very strong signals (similar to 20,000 cps). It was therefore very clear which samples had been in the CT scanner. For comparison, the natural TL signal from Antarctic meteorites is similar to 5000-50,000 cps. Using the methods developed for Antarctic meteorites, the apparent dose absorbed by the five test samples was calculated to be 83 +/- 5 krad, comparable with the highest doses observed in Antarctic meteorites and freshly fallen meteorites. While these results do not preclude the use of CT scanners when scientifically justified, it should be remembered that the record of radiation exposure to ionizing radiations for the sample will be destroyed and that TL, or the related optically stimulated luminescence, are the primary modern techniques for radiation dosimetry. This is particularly important with irreplaceable samples, such as meteorite main masses, returned samples, and samples destined for archive.
C1 [Sears, Derek W. G.; Sears, Hazel] NASA, Ames Res Ctr, BAER Inst, Mountain View, CA 95035 USA.
[Ebel, Denton S.; Wallace, Sean; Friedrich, Jon M.] Amer Museum Nat Hist, New York, NY 10024 USA.
[Friedrich, Jon M.] Fordham Univ, Dept Chem, New York, NY 10458 USA.
RP Sears, DWG (reprint author), NASA, Ames Res Ctr, BAER Inst, Mountain View, CA 95035 USA.
EM derek.sears@nasa.gov
NR 20
TC 0
Z9 0
U1 5
U2 6
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD APR
PY 2016
VL 51
IS 4
BP 833
EP 838
DI 10.1111/maps.12622
PG 6
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DJ2QT
UT WOS:000374050800013
ER
PT J
AU Wiley, PE
Trent, JD
AF Wiley, Patrick E.
Trent, Jonathan D.
TI Clarification of algae-laden water using electrochemical processes
SO WATER SCIENCE AND TECHNOLOGY-WATER SUPPLY
LA English
DT Article
DE algae; disinfection; drinking water; electrocoagulation;
electroflotation
ID WASTE-WATER; DRINKING-WATER; ELECTROCOAGULATION; COAGULATION; REMOVAL;
POLLUTANTS; GENERATION; ELECTRODES; SEPARATION; FLOTATION
AB Algae contamination of surface water and drinking water supplies is a significant problem particularly in rural areas. A decentralized inexpensive technology that would effectively remove algae from water would be beneficial. Electrocoagulation (EC) combined with electroflotation (EF) as a single process (ECF) is a promising algae harvesting technique with no moving parts that may be powered using a modest array of photovoltaic panels if a low power system can be developed. Here, an ECF system was constructed to study the energy required to remove algae from a simulated drinking water supply. Results from 18 ECF experiments indicated a >95% improvement of water clarity measured by optical density (OD750) could be achieved with as little energy as 1.25 kWh m(-3). The key was to find the ideal combination of gas bubbles produced by EF (G) and coagulant from the EC relative to the concentration of suspended solids (S). The ideal gas to solids (G/S) ratio for the ECF system ranged from 0.09 to 0.17. In solutions containing chloride (Cl-) ions ECF produced chlorine gas which is known to contribute to disinfection. Results suggest that ECF can efficiently remove algae and simultaneously contribute to disinfecting contaminated drinking water supplies.
C1 [Wiley, Patrick E.] Kennebunk Sewer Dist, 71 Water St, Kennebunk, ME 04043 USA.
[Trent, Jonathan D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Wiley, PE (reprint author), Kennebunk Sewer Dist, 71 Water St, Kennebunk, ME 04043 USA.
EM pwiley@ksdistrict.org
FU University of California, Merced; PERC Water; NASA Ames Research Center
GSRP
FX The authors acknowledge Professor Elliott Campbell from the University
of California, Merced, Brian Cullen and Nate Owen from PERC Water, and
the NASA Ames Research Center GSRP for providing financial support.
NR 29
TC 0
Z9 0
U1 7
U2 15
PU IWA PUBLISHING
PI LONDON
PA ALLIANCE HOUSE, 12 CAXTON ST, LONDON SW1H0QS, ENGLAND
SN 1606-9749
J9 WATER SCI TECH-W SUP
JI Water Sci. Technol.-Water Supply
PD APR
PY 2016
VL 16
IS 2
BP 314
EP 323
DI 10.2166/ws.2015.140
PG 10
WC Engineering, Environmental; Environmental Sciences; Water Resources
SC Engineering; Environmental Sciences & Ecology; Water Resources
GA DJ6FF
UT WOS:000374305100006
ER
PT J
AU Schreiner, SS
Sibille, L
Dominguez, JA
Hoffman, JA
AF Schreiner, Samuel S.
Sibille, Laurent
Dominguez, Jesus A.
Hoffman, Jeffrey A.
TI A parametric sizing model for Molten Regolith Electrolysis reactors to
produce oxygen on the Moon
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Molten Regolith Electrolysis; In situ resource utilization; Lunar oxygen
production; Moon; Molten oxide electrolysis; Parametric modeling
ID ELECTROCHEMICAL REDUCTION; LUNAR REGOLITH; DESIGN; METAL; TITANIUM;
ANODE; OXIDE; IRON
AB We present a parametric sizing model for a Molten Regolith Electrolysis (MRE) reactor that produces oxygen and molten metals from lunar regolith. The model has a foundation of regolith material property models validated using data from Apollo samples and simulants. A multiphysics simulation of an MRE reactor is developed and leveraged to generate a database linking reactor design and performance trends. A novel design methodology is created which utilizes this database to parametrically design an MRE reactor that can (1) sustain the required current, operating temperature, and mass of molten regolith to meet a desired oxygen production level, (2) operate for long periods of time by protecting the reactor walls from the corrosive molten regolith with a layer of solid "frozen" regolith, and (3) support a range of electrode separations to enable operational flexibility. Mass, power, and performance estimates for an MRE reactor are presented for a range of oxygen production levels. Sensitivity analyses are presented for several design variables, including operating temperature, regolith feedstock composition, and the degree of operational flexibility. (c) 2016 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Schreiner, Samuel S.; Hoffman, Jeffrey A.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Sibille, Laurent; Dominguez, Jesus A.] NASA, Kennedy Space Ctr, FL 32899 USA.
[Schreiner, Samuel S.] MIT, Dept Aeronaut & Astronaut, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Sibille, Laurent] NASA, Surface Syst Grp, ESC-5, Kennedy Space Ctr, FL 32899 USA.
[Dominguez, Jesus A.] NASA, VENCORE ESC, Kennedy Space Ctr, FL 32899 USA.
[Hoffman, Jeffrey A.] MIT, Dept Aeronaut & Astronaut, Practice, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
RP Schreiner, SS (reprint author), MIT, Dept Aeronaut & Astronaut, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM schr0910@umn.edu
FU NASA Space Technology Research Fellowship [NNX13AL76H]
FX This work was supported by a NASA Space Technology Research Fellowship
(Grant #NNX13AL76H). Any opinions, findings, and conclusions or
recommendations expressed in this material are those of the author and
do not necessarily reflect the views of NASA.
NR 59
TC 0
Z9 0
U1 4
U2 5
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 1
PY 2016
VL 57
IS 7
BP 1585
EP 1603
DI 10.1016/j.asr.2016.01.006
PG 19
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA DI5OY
UT WOS:000373549700012
ER
PT J
AU Walker, M
Venable, D
Whiteman, DN
Sakai, T
AF Walker, Monique
Venable, Demetrius
Whiteman, David N.
Sakai, Tetsu
TI Application of the lamp mapping technique for overlap function for Raman
lidar systems
SO APPLIED OPTICS
LA English
DT Article
ID WATER-VAPOR; RECEIVER; SIGNALS
AB Traditionally, the lidar water vapor mixing ratio (WVMR) is corrected for overlap using data from another instrument, such as a radiosonde. Here we introduce a new experimental method to determine the overlap function using the lamp mapping technique (LMT), which relies on the lidar optics and detection system. The LMT discussed here involves a standard halogen lamp being scanned over the aperture of a Raman lidar telescope in synchronization with the lidar detection system [Appl. Opt. 50, 4622 (2011), Appl. Opt. 53, 8538 (2014)]. In this paper, we show results for a LMT-determined overlap function for individual channels, as well as a WVMR overlap function. We found that the LMT-determined WVMR overlap functions deviate within 5% of the traditional radiosonde-determined overlap. (C) 2016 Optical Society of America
C1 [Walker, Monique] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21044 USA.
[Walker, Monique; Whiteman, David N.] NASA, Goddard Space Flight Ctr, Mesoscale & Atmospher Proc, Greenbelt, MD 20771 USA.
[Venable, Demetrius] Howard Univ, Dept Phys & Astron, Washington, DC 20059 USA.
[Sakai, Tetsu] Meteorol Res Inst, 1-1 Nagamine, Tsukuba, Ibaraki 305, Japan.
RP Walker, M (reprint author), Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21044 USA.; Walker, M (reprint author), NASA, Goddard Space Flight Ctr, Mesoscale & Atmospher Proc, Greenbelt, MD 20771 USA.
EM Monique.N.Walker@Nasa.gov
FU National Aeronautics and Space Administration (NASA) Atmospheric
Composition program
FX National Aeronautics and Space Administration (NASA) Atmospheric
Composition program.
NR 16
TC 0
Z9 0
U1 4
U2 4
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD APR 1
PY 2016
VL 55
IS 10
BP 2551
EP 2558
DI 10.1364/AO.55.002551
PG 8
WC Optics
SC Optics
GA DI3LS
UT WOS:000373400800013
PM 27139656
ER
PT J
AU Kim, MK
Lau, WKM
Kim, KM
Sang, J
Kim, YH
Lee, WS
AF Kim, Maeng-Ki
Lau, William K. M.
Kim, Kyu-Myong
Sang, Jeong
Kim, Yeon-Hee
Lee, Woo-Seop
TI Amplification of ENSO effects on Indian summer monsoon by absorbing
aerosols
SO CLIMATE DYNAMICS
LA English
DT Article
DE EHP; Monsoon; ENSO; Absorbing aerosol; Dust; Black carbon
ID BLACK CARBON AEROSOLS; ANTHROPOGENIC AEROSOLS; SATELLITE MEASUREMENTS;
OCEAN DIPOLE; VARIABILITY; RAINFALL; TELECONNECTION; PRECIPITATION;
RADIATION; ONSET
AB In this study, we present observational evidence, based on satellite aerosol measurements and MERRA reanalysis data for the period 1979-2011, indicating that absorbing aerosols can have strong influence on seasonal-to-interannual variability of the Indian summer monsoon rainfall, including amplification of ENSO effects. We find a significant correlation between ENSO (El Nino Southern Oscillation) and aerosol loading in AprilMay, with La Nina (El Nino) conditions favoring increased (decreased) aerosol accumulation over northern India, with maximum aerosol optical depth over the Arabian Sea and Northwestern India, indicative of strong concentration of dust aerosols transported from West Asia and Middle East deserts. Composite analyses based on a normalized aerosol index (NAI) show that high concentration of aerosol over northern India in April-May is associated with increased moisture transport, enhanced dynamically induced warming of the upper troposphere over the Tibetan Plateau, and enhanced rainfall over northern India and the Himalayan foothills during May-June, followed by a subsequent suppressed monsoon rainfall over all India, consistent with the elevated heat pump (EHP) hypothesis (Lau et al. in Clim Dyn 26: 855-864, 2006. doi: 10.1007/s00382-006-0114-z). Further analyses from sub-sampling of ENSO years, with normal (<1-sigma), and abnormal (>1-sigma) NAI over northern India respectively show that the EHP may lead to an amplification of the Indian summer monsoon response to ENSO forcing, particularly with respect to the increased rainfall over the Himalayan foothills, and the warming of the upper troposphere over the Tibetan Plateau. Our results suggest that absorbing aerosol, particular desert dusts can strongly modulate ENSO influence, and possibly play important roles as a feedback agent in climate change in Asian monsoon regions.
C1 [Kim, Maeng-Ki; Sang, Jeong] Kongju Natl Univ, Dept Atmospher Sci, Kong Ju 314701, South Korea.
[Lau, William K. M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Kim, Kyu-Myong] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Kim, Yeon-Hee] Pohang Univ Sci & Technol POSTECH, Sch Environm Sci & Engn, Pohang 790784, Gyeongbuk, South Korea.
[Lee, Woo-Seop] APEC Climate Ctr, Busan 612020, South Korea.
RP Kim, MK (reprint author), Kongju Natl Univ, Dept Atmospher Sci, Kong Ju 314701, South Korea.
EM mkkim@kongju.ac.kr
FU Korea Meteorological Administration Research and Development Program
[KMIPA2015-2085]; GSFC Strategic Science Support; NASA Interdisciplinary
(IDS) Investigations
FX This work was funded by the Korea Meteorological Administration Research
and Development Program under Grant KMIPA2015-2085. Partial support was
provided by the GSFC Strategic Science Support, and the NASA
Interdisciplinary (IDS) Investigations.
NR 66
TC 9
Z9 9
U1 8
U2 25
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD APR
PY 2016
VL 46
IS 7-8
BP 2657
EP 2671
DI 10.1007/s00382-015-2722-y
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DI4AR
UT WOS:000373442900036
ER
PT J
AU Margulis, SA
Cortes, G
Girotto, M
Durand, M
AF Margulis, Steven A.
Cortes, Gonzalo
Girotto, Manuela
Durand, Michael
TI A Landsat-Era Sierra Nevada Snow Reanalysis (1985-2015)
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Physical Meteorology and Climatology; Snowpack; Data assimilation;
Observational techniques and algorithms; Geographic location/entity;
Bayesian methods; Mathematical and statistical techniques; Remote
sensing; Atm/Ocean Structure/ Phenomena; Models and modeling; Complex
terrain
ID WATER EQUIVALENT; COVER; PRECIPITATION; ACCUMULATION; ASSIMILATION;
CALIFORNIA; RESOURCES; HYDROLOGY; CLIMATE; REGION
AB A newly developed state-of-the-art snow water equivalent (SWE) reanalysis dataset over the Sierra Nevada (United States) based on the assimilation of remotely sensed fractional snow-covered area data over the Landsat 5-8 record (1985-2015) is presented. The method (fully Bayesian), resolution (daily and 90 m), temporal extent (31 years), and accuracy provide a unique dataset for investigating snow processes. The verified dataset (based on a comparison with over 9000 station years of in situ data) exhibited mean and root-mean-square errors less than 3 and 13 cm, respectively, and correlation greater than 0.95 compared with in situ SWE observations. The reanalysis dataset was used to characterize the peak SWE climatology to provide a basic accounting of the stored snowpack water in the Sierra Nevada over the last 31 years. The pixel-wise peak SWE volume over the domain was found to be 20.0 km(3) on average with a range of 4.0-40.6 km(3). The ongoing drought in California contains the two lowest snowpack years (water years 2014 and 2015) and three of the four driest years over the examined record. It was found that the basin-average peak SWE, while underestimating the total water storage in snowpack over the year, accurately captures the interannual variability in stored snowpack water. However, the results showed that the assumption that 1 April SWE is representative of the peak SWE can lead to significant underestimation of basin-average peak SWE both on an average (21% across all basins) and on an interannual basis (up to 98% across all basin years).
C1 [Margulis, Steven A.; Cortes, Gonzalo] Univ Calif Los Angeles, Dept Civil & Environm Engn, 5732D Boelter Hall, Los Angeles, CA 90095 USA.
[Girotto, Manuela] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Girotto, Manuela] Univ Space Res Assoc, GESTAR, Columbia, MD USA.
[Durand, Michael] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
[Durand, Michael] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
RP Margulis, SA (reprint author), Univ Calif Los Angeles, Dept Civil & Environm Engn, 5732D Boelter Hall, Los Angeles, CA 90095 USA.
EM margulis@seas.ucla.edu
FU NASA NEWS project [NNX15AD16G]; NASA Earth System Science Fellowship
[NNX11AL58H]; National Science Foundation [EAR-1246473]
FX This work was based in part upon work supported by a NASA NEWS project
(Grant NNX15AD16G), a NASA Earth System Science Fellowship (Grant
NNX11AL58H), and the National Science Foundation (Grant EAR-1246473).
The NLDAS-2 data used in this study were acquired as part of the mission
of NASA's Earth Science Division and were archived and distributed by
the Goddard Earth Sciences (GES) Data and Information Services Center
(DISC). The raw Landsat data were obtained from the USGS Earth Explorer
Landsat archive (http://earthexplorer.usgs.gov/).
NR 40
TC 3
Z9 3
U1 2
U2 12
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD APR
PY 2016
VL 17
IS 4
BP 1203
EP 1221
DI 10.1175/JHM-D-15-0177.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DI7FZ
UT WOS:000373666000001
ER
PT J
AU Mishchenko, MI
Dlugach, JM
Zakharova, NT
AF Mishchenko, Michael I.
Dlugach, Janna M.
Zakharova, Nadezhda T.
TI Demonstration of numerical equivalence of ensemble and spectral
averaging in electromagnetic scattering by random particulate media
SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA A-OPTICS IMAGE SCIENCE AND
VISION
LA English
DT Article
ID WEAK-LOCALIZATION; LIGHT-SCATTERING; T-MATRIX; PARTICLES; SPHERES
AB The numerically exact superposition T-matrix method is used to model far-field electromagnetic scattering by two types of particulate object. Object 1 is a fixed configuration that consists of N identical spherical particles (with N = 200 or 400) quasi-randomly populating a spherical volume V having a median size parameter of 50. Object 2 is a true discrete random medium (DRM) comprising the same number N of particles randomly moving throughout V. The median particle size parameter is fixed at 4. We show that if Object 1 is illuminated by a quasi-monochromatic parallel beam then it generates a typical speckle pattern having no resemblance to the scattering pattern generated by Object 2. However, if Object 1 is illuminated by a parallel polychromatic beam with a 10% bandwidth then it generates a scattering pattern that is largely devoid of speckles and closely reproduces the quasi-monochromatic pattern generated by Object 2. This result serves to illustrate the capacity of the concept of electromagnetic scattering by a DRM to encompass fixed quasi-random particulate samples provided that they are illuminated by polychromatic light. (C) 2016 Optical Society of America
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Dlugach, Janna M.] Natl Acad Sci Ukraine, Main Astron Observ, 27 Zabolotny Str, UA-03680 Kiev, Ukraine.
[Zakharova, Nadezhda T.] Trinnovim LLC, 2880 Broadway, New York, NY 10025 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM michael.i.mishchenko@nasa.gov
FU NASA Remote Sensing Theory Program; National Academy of Sciences of
Ukraine (Main Astronomical Observatory GRAPE/GPU/GRID Computing Cluster
Project)
FX NASA Remote Sensing Theory Program; National Academy of Sciences of
Ukraine (Main Astronomical Observatory GRAPE/GPU/GRID Computing Cluster
Project).
NR 27
TC 2
Z9 2
U1 0
U2 2
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1084-7529
EI 1520-8532
J9 J OPT SOC AM A
JI J. Opt. Soc. Am. A-Opt. Image Sci. Vis.
PD APR 1
PY 2016
VL 33
IS 4
BP 618
EP 624
DI 10.1364/JOSAA.33.000618
PG 7
WC Optics
SC Optics
GA DI3KU
UT WOS:000373398300024
PM 27140771
ER
PT J
AU Lundkvist, MS
Kjeldsen, H
Albrecht, S
Davies, GR
Basu, S
Huber, D
Justesen, AB
Karoff, C
Aguirre, VS
Van Eylen, V
Vang, C
Arentoft, T
Barclay, T
Bedding, TR
Campante, TL
Chaplin, WJ
Christensen-Dalsgaard, J
Elsworth, YP
Gilliland, RL
Handberg, R
Hekker, S
Kawaler, SD
Lund, MN
Metcalfe, TS
Miglio, A
Rowe, JF
Stello, D
Tingley, B
White, TR
AF Lundkvist, M. S.
Kjeldsen, H.
Albrecht, S.
Davies, G. R.
Basu, S.
Huber, D.
Justesen, A. B.
Karoff, C.
Aguirre, V. Silva
Van Eylen, V.
Vang, C.
Arentoft, T.
Barclay, T.
Bedding, T. R.
Campante, T. L.
Chaplin, W. J.
Christensen-Dalsgaard, J.
Elsworth, Y. P.
Gilliland, R. L.
Handberg, R.
Hekker, S.
Kawaler, S. D.
Lund, M. N.
Metcalfe, T. S.
Miglio, A.
Rowe, J. F.
Stello, D.
Tingley, B.
White, T. R.
TI Hot super-Earths stripped by their host stars
SO NATURE COMMUNICATIONS
LA English
DT Article
ID FALSE-POSITIVE RATE; KEPLER PLANET CANDIDATES; SOLAR-TYPE STARS; RADIUS
DISTRIBUTION; FUNDAMENTAL PROPERTIES; LIGHT-CURVE; GIANT STARS;
ASTEROSEISMOLOGY; SYSTEMS; MASS
AB Simulations predict that hot super-Earth sized exoplanets can have their envelopes stripped by photoevaporation, which would present itself as a lack of these exoplanets. However, this absence in the exoplanet population has escaped a firm detection. Here we demonstrate, using asteroseismology on a sample of exoplanets and exoplanet candidates observed during the Kepler mission that, while there is an abundance of super-Earth sized exoplanets with low incident fluxes, none are found with high incident fluxes. We do not find any exoplanets with radii between 2.2 and 3.8 Earth radii with incident flux above 650 times the incident flux on Earth. This gap in the population of exoplanets is explained by evaporation of volatile elements and thus supports the predictions. The confirmation of a hot-super-Earth desert caused by evaporation will add an important constraint on simulations of planetary systems, since they must be able to reproduce the dearth of close-in super-Earths.
C1 [Lundkvist, M. S.; Kjeldsen, H.; Albrecht, S.; Davies, G. R.; Huber, D.; Justesen, A. B.; Karoff, C.; Aguirre, V. Silva; Van Eylen, V.; Vang, C.; Arentoft, T.; Bedding, T. R.; Campante, T. L.; Chaplin, W. J.; Christensen-Dalsgaard, J.; Elsworth, Y. P.; Handberg, R.; Hekker, S.; Lund, M. N.; Metcalfe, T. S.; Miglio, A.; Stello, D.; Tingley, B.; White, T. R.] Aarhus Univ, Dept Phys & Astron, SAC, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
[Lundkvist, M. S.] Heidelberg Univ, Zentrum Astron, Konigstuhl 12, D-69117 Heidelberg, Germany.
[Davies, G. R.; Campante, T. L.; Chaplin, W. J.; Elsworth, Y. P.; Lund, M. N.; Miglio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Basu, S.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Huber, D.; Bedding, T. R.; Stello, D.] Univ Sydney, Sch Phys, SIfA, Sydney, NSW 2006, Australia.
[Karoff, C.] Aarhus Univ, Dept Geosci, Hoegh Guldbergs Gade 2, DK-8000 Aarhus C, Denmark.
[Barclay, T.; Rowe, J. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, T.] Bay Area Environm Res Inst, 596 1st St West, Sonoma, CA 95476 USA.
[Gilliland, R. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, 525 Davey Lab, University Pk, PA 16802 USA.
[Hekker, S.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
[Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Metcalfe, T. S.] Space Sci Inst, Boulder, CO 80301 USA.
[Rowe, J. F.] SETI Inst, Mountain View, CA 94043 USA.
[White, T. R.] Univ Gottingen, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany.
RP Lundkvist, MS (reprint author), Aarhus Univ, Dept Phys & Astron, SAC, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.; Lundkvist, MS (reprint author), Heidelberg Univ, Zentrum Astron, Konigstuhl 12, D-69117 Heidelberg, Germany.
EM lundkvist@phys.au.dk
OI Lundkvist, Mia Sloth/0000-0002-8661-2571; Karoff,
Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661;
Handberg, Rasmus/0000-0001-8725-4502; Lund, Mikkel
Norup/0000-0001-9214-5642
FU Danish National Research Foundation [DNRF106]; ASTERISK project -
European Research Council [267864]
FX Funding for the Stellar Astrophysics Centre is provided by The Danish
National Research Foundation (Grant agreement no.: DNRF106). The
research is supported by the ASTERISK project (ASTERoseismic
Investigations with SONG and Kepler) funded by the European Research
Council (Grant agreement no.: 267864). This research has made use of
NASA's Astrophysics Data System and the NASA Exoplanet Archive, which is
operated by the California Institute of Technology, under contract with
the National Aeronautics and Space Administration under the Exoplanet
Exploration Program.
NR 53
TC 7
Z9 7
U1 0
U2 0
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD APR
PY 2016
VL 7
AR 11201
DI 10.1038/ncomms11201
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DI9MA
UT WOS:000373825700001
PM 27062914
ER
PT J
AU Saglamyurek, E
Puigibert, MG
Zhou, Q
Giner, L
Marsili, F
Verma, VB
Nam, SW
Oesterling, L
Nippa, D
Oblak, D
Tittel, W
AF Saglamyurek, Erhan
Puigibert, Marcelli Grimau
Zhou, Qiang
Giner, Lambert
Marsili, Francesco
Verma, Varun B.
Nam, Sae Woo
Oesterling, Lee
Nippa, David
Oblak, Daniel
Tittel, Wolfgang
TI A multiplexed light-matter interface for fibre-based quantum networks
SO NATURE COMMUNICATIONS
LA English
DT Article
ID MEMORY; STORAGE; PHOTONS
AB Processing and distributing quantum information using photons through fibre-optic or free-space links are essential for building future quantum networks. The scalability needed for such networks can be achieved by employing photonic quantum states that are multiplexed into time and/or frequency, and light-matter interfaces that are able to store and process such states with large time-bandwidth product and multimode capacities. Despite important progress in developing such devices, the demonstration of these capabilities using non-classical light remains challenging. Here, employing the atomic frequency comb quantum memory protocol in a cryogenically cooled erbium-doped optical fibre, we report the quantum storage of heralded single photons at a telecom-wavelength (1.53 mu m) with a time-bandwidth product approaching 800. Furthermore, we demonstrate frequency-multimode storage and memory-based spectral-temporal photon manipulation. Notably, our demonstrations rely on fully integrated quantum technologies operating at telecommunication wavelengths. With improved storage efficiency, our light-matter interface may become a useful tool in future quantum networks.
C1 [Saglamyurek, Erhan; Puigibert, Marcelli Grimau; Zhou, Qiang; Giner, Lambert; Oblak, Daniel; Tittel, Wolfgang] Univ Calgary, Inst Quantum Sci & Technol, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada.
[Saglamyurek, Erhan; Puigibert, Marcelli Grimau; Zhou, Qiang; Giner, Lambert; Oblak, Daniel; Tittel, Wolfgang] Univ Calgary, Dept Phys & Astron, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada.
[Marsili, Francesco] CALTECH, Jet Prop Lab, Div Appl Phys, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Verma, Varun B.; Nam, Sae Woo] NIST, Boulder, CO 80305 USA.
[Oesterling, Lee; Nippa, David] Battelle Mem Inst, 505 King Ave, Columbus, OH 43201 USA.
[Giner, Lambert] Univ Ottawa, Dept Phys, 150 Louis Pasteur, Ottawa, ON K1N 6N5, Canada.
RP Tittel, W (reprint author), Univ Calgary, Inst Quantum Sci & Technol, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada.; Tittel, W (reprint author), Univ Calgary, Dept Phys & Astron, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada.
EM wtittel@ucalgary.ca
RI Tittel, Wolfgang/A-1600-2011
FU Alberta Innovates Technology Futures; National Science and Engineering
Research Council of Canada; Canadian Institute for Advanced Research;
DARPA Information in a Photon (InPho) programme; National Aeronautics
and Space Administration
FX E.S., M.G., Q.Z., L.G., D.O. and W.T. thank Jeongwan Jin, Neil Sinclair,
Charles Thiel and Vladimir Kiselyov for discussions and technical
support, and acknowledge funding through the Alberta Innovates
Technology Futures and the National Science and Engineering Research
Council of Canada. Furthermore, W.T. acknowledges support as a Senior
Fellow of the Canadian Institute for Advanced Research, and V.B.V. and
S.W.N. partial funding for detector development from the DARPA
Information in a Photon (InPho) programme. Part of the research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. L.O. and D.N. acknowledge Srico Inc. for their
assistance with the fabrication of PPLN wafers.
NR 37
TC 1
Z9 1
U1 17
U2 30
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD APR
PY 2016
VL 7
AR 11202
DI 10.1038/ncomms11202
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DI6PK
UT WOS:000373621700001
PM 27046076
ER
PT J
AU Cataldo, G
Wollack, EJ
Brown, AD
Miller, KH
AF Cataldo, Giuseppe
Wollack, Edward J.
Brown, Ari D.
Miller, Kevin H.
TI Infrared dielectric properties of low-stress silicon oxide
SO OPTICS LETTERS
LA English
DT Article
ID OPTICAL-PROPERTIES; FREQUENCY-DEPENDENCE; THIN-FILMS; ABSORPTION;
NITRIDE; GLASS; SUBMILLIMETER; TEMPERATURE; MILLIMETER; SPECTRA
AB Silicon oxide thin films play an important role in the realization of optical coatings and high-performance electrical circuits. Estimates of the dielectric function in the farand mid-infrared regime are derived from the observed transmittance spectrum for a commonly employed lowstress silicon oxide formulation. The experimental, modeling, and numerical methods used to extract the dielectric function are presented. (C) 2016 Optical Society of America
C1 [Cataldo, Giuseppe; Wollack, Edward J.; Brown, Ari D.; Miller, Kevin H.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Cataldo, G (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Giuseppe.Cataldo@NASA.gov
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
FU National Aeronautics and Space Administration (NASA)
[NNH12ZDA001N-APRA]; Goddard Space Flight Center (GSFC) (Internal
Research and Development)
FX National Aeronautics and Space Administration (NASA)
(NNH12ZDA001N-APRA); Goddard Space Flight Center (GSFC) (Internal
Research and Development).
NR 33
TC 3
Z9 3
U1 1
U2 5
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
EI 1539-4794
J9 OPT LETT
JI Opt. Lett.
PD APR 1
PY 2016
VL 41
IS 7
BP 1364
EP 1367
DI 10.1364/OL.41.001364
PG 4
WC Optics
SC Optics
GA DI0ZI
UT WOS:000373225400015
PM 27192237
ER
PT J
AU Berninger, JP
LaLone, CA
Villeneuve, DL
Ankley, GT
AF Berninger, Jason P.
LaLone, Carlie A.
Villeneuve, Daniel L.
Ankley, Gerald T.
TI PRIORITIZATION OF PHARMACEUTICALS FOR POTENTIAL ENVIRONMENTAL HAZARD
THROUGH LEVERAGING A LARGE-SCALE MAMMALIAN PHARMACOLOGICAL DATASET
SO ENVIRONMENTAL TOXICOLOGY AND CHEMISTRY
LA English
DT Article
DE Pharmaceuticals; Risk ranking; Hazard/risk assessment
ID PERSONAL CARE PRODUCTS; RISK-ASSESSMENT; VETERINARY MEDICINES; AQUATIC
ORGANISMS; FISH; ECOTOXICOLOGY; SUBSTANCES; RANKING; ANTIDEPRESSANTS;
EXTRAPOLATION
AB The potential for pharmaceuticals in the environment to cause adverse ecological effects is of increasing concern. Given the thousands of active pharmaceutical ingredients (APIs) that can enter the aquatic environment through human and/or animal (e.g., livestock) waste, a current challenge in aquatic toxicology is identifying those that pose the greatest risk. Because empirical toxicity information for aquatic species is generally lacking for pharmaceuticals, an important data source for prioritization is that generated during the mammalian drug development process. Applying concepts of species read-across, mammalian pharmacokinetic data were used to systematically prioritize APIs by estimating their potential to cause adverse biological consequences to aquatic organisms, using fish as an example. Mammalian absorption, distribution, metabolism, and excretion (ADME) data (e.g., peak plasma concentration, apparent volume of distribution, clearance rate, and half-life) were collected and curated, creating the Mammalian Pharmacokinetic Prioritization For Aquatic Species Targeting (MaPPFAST) database representing 1070 APIs. From these data, a probabilistic model and scoring system were developed and evaluated. Individual APIs and therapeutic classes were ranked based on clearly defined read-across assumptions for translating mammalian-derived ADME parameters to estimate potential hazard in fish (i.e., greatest predicted hazard associated with lowest mammalian peak plasma concentrations, total clearance and highest volume of distribution, half-life). It is anticipated that the MaPPFAST database and the associated API prioritization approach will help guide research and/or inform ecological risk assessment. Published 2015 Wiley Periodicals Inc. on behalf of SETAC. This article is a US Government work and, as such, is in the public domain in the United States of America.
C1 [Berninger, Jason P.] US EPA, Natl Res Council, Duluth, MN USA.
[LaLone, Carlie A.] Univ Minnesota, Water Resources Ctr, Coll Food Agr & Nat Resource Sci, St Paul, MN 55108 USA.
[LaLone, Carlie A.; Villeneuve, Daniel L.; Ankley, Gerald T.] US EPA, Off Res & Dev, Natl Hlth & Environm Effects Res Lab, Midcontinent Ecol Div, Duluth, MN USA.
RP Berninger, JP (reprint author), US EPA, Natl Res Council, Duluth, MN USA.
EM JasonBerninger@gmail.com
RI Berninger, Jason/O-2401-2016
OI Berninger, Jason/0000-0003-3045-7899
NR 62
TC 3
Z9 3
U1 8
U2 33
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0730-7268
EI 1552-8618
J9 ENVIRON TOXICOL CHEM
JI Environ. Toxicol. Chem.
PD APR
PY 2016
VL 35
IS 4
BP 1007
EP 1020
DI 10.1002/etc.2965
PG 14
WC Environmental Sciences; Toxicology
SC Environmental Sciences & Ecology; Toxicology
GA DH0RB
UT WOS:000372490300027
PM 25772004
ER
PT J
AU Kritzer, JP
Delucia, MB
Greene, E
Shumway, C
Topolski, MF
Thomas-Blate, J
Chiarella, LA
Davy, KB
Smith, K
AF Kritzer, Jacob P.
Delucia, Mari-Beth
Greene, Emily
Shumway, Caroly
Topolski, Marek F.
Thomas-Blate, Jessie
Chiarella, Louis A.
Davy, Kay B.
Smith, Kent
TI The Importance of Benthic Habitats for Coastal Fisheries
SO BIOSCIENCE
LA English
DT Article
DE coastal ecosystems; fisheries; marine biology; aquatic ecosystems;
conservation
ID ECOSYSTEM SERVICES; FISH COMMUNITIES; MANAGEMENT; ESTUARINE; JUVENILE;
IMPACTS; CONSERVATION; BIODIVERSITY; CONNECTIVITY; ASSEMBLAGES
AB Ecosystem-based management requires greater attention to habitat conservation. We evaluate the importance of benthic habitats as space for shelter, feeding, and breeding by coastal fishes and motile invertebrates in four biogeographic regions of the eastern United States. The importance of different habitats changed with latitude. Soft sediments and riverine systems scored higher in northern regions, and marshes and coral reefs scored higher in the south. The importance of soft sediments is notable because environmental assessments often assume their ecological value is lower. Submerged aquatic vegetation was a key nursery habitat coast-wide. An important consideration is that anthropogenic impacts have altered habitat availability and use, and climate change is causing ongoing disturbance. Furthermore, distinct habitats should not be managed in isolation but rather as interconnected mosaics. Our approach, combined with information on status, vulnerability, and other ecological functions, can be used to evaluate trade-offs and develop habitat-management strategies.
C1 [Kritzer, Jacob P.] Environm Def Fund, Boston, MA USA.
[Delucia, Mari-Beth] Nature Conservancy, Harrisburg, PA USA.
[Greene, Emily] Earth Resources Technol Inc, Laurel, MD USA.
[Shumway, Caroly] Merrimack River Watershed Council, Lawrence, MA USA.
[Topolski, Marek F.] Maryland Dept Nat Resources, Fisheries Serv, Annapolis, MD USA.
[Thomas-Blate, Jessie] Amer Rivers, Washington, DC USA.
[Chiarella, Louis A.] Natl Marine Fisheries Serv, Greater Atlant Reg Fisheries Off, Gloucester, MA USA.
[Davy, Kay B.] Natl Marine Fisheries Serv, Protected Resources Div, Dania, FL USA.
[Smith, Kent] Florida Fish & Wildlife Conservat Commiss, Aquat Habitat Conservat & Restorat Sect, Tallahassee, FL USA.
RP Kritzer, JP (reprint author), Environm Def Fund, Boston, MA USA.
EM jkritzer@edf.org
FU ASMFC; ACFHP [DC M-60-HM]; USFWS [F14AC00728]
FX We thank the many scientists at agencies, institutions, and
organizations along the Atlantic coast that completed - sections of the
matrix, participated in review meetings, or conducted independent
reviews (see the supplementary material for a full list). Funding for
the habitat evaluation was provided to ASMFC and ACFHP through the
Multistate Conservation Grant Program, grant no. DC M-60-HM,
administered by the U.S. Fish and Wildlife Agency (USFWS) and the
Association of Fish and Wildlife Agencies. Additional funding was
provided by USFWS cooperative agreement no. F14AC00728 to ASMFC.
Comments from three anonymous reviewers improved the quality of this
article, although the content remains the sole responsibility of the
authors. The habitat scores and supporting bibliography are archived by
ACFHP (www.atlanticfishhabitat.org). The authors claim no conflicts of
interest.
NR 64
TC 1
Z9 1
U1 8
U2 30
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0006-3568
EI 1525-3244
J9 BIOSCIENCE
JI Bioscience
PD APR
PY 2016
VL 66
IS 4
BP 274
EP 284
DI 10.1093/biosci/biw014
PG 11
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA DI0WK
UT WOS:000373217800004
ER
PT J
AU Leroux, DJ
Das, NN
Entekhabi, D
Colliander, A
Njoku, E
Jackson, TJ
Yueh, S
AF Leroux, Delphine J.
Das, Narendra N.
Entekhabi, Dara
Colliander, Andreas
Njoku, Eni
Jackson, Thomas J.
Yueh, Simon
TI Active-Passive Soil Moisture Retrievals During the SMAP Validation
Experiment 2012
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Active-passive; brightness temperature disaggregation; SMAP; soil
moisture
ID RADIOMETER; SMAPVEX12; RADAR
AB The goal of this study is to assess the performance of the active-passive algorithm for the NASA Soil Moisture Active Passive mission (SMAP) using airborne and ground observations from a field campaign. The SMAP active-passive algorithm disaggregates the coarse-resolution radiometer brightness temperature (TB) using high-resolution radar backscatter (sigma(o)) observations. The colocated TB and sigma(o) acquired by the aircraft-based Passive Active L-and S-band sensor during the SMAP Validation Experiment 2012 (SMAPVEX12) are used to evaluate this algorithm. The estimation of its parameters is affected by changes in vegetation during the campaign. Key features of the campaign were the wide range of vegetation growth and soil moisture conditions during the experiment period. The algorithm performance is evaluated by comparing retrieved soil moisture from the disaggregated brightness temperatures to in situ soil moisture measurements. A minimum performance algorithm is also applied, where the radar data are withheld. The minimum performance algorithm serves as a benchmark to asses the value of the radar to the SMAP active-passive algorithm. The temporal correlation between ground samples and the SMAP active-passive algorithm is improved by 21% relative to minimum performance. The unbiased root-mean-square error is decreased by 15% overall.
C1 [Leroux, Delphine J.; Das, Narendra N.; Colliander, Andreas; Njoku, Eni; Yueh, Simon] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Leroux, Delphine J.] Ctr Etud Spatiales Biosphere CESBIO, F-31400 Toulouse, France.
[Entekhabi, Dara] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Jackson, Thomas J.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA.
RP Das, NN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM nndas@jpl.nasa.gov
NR 12
TC 4
Z9 4
U1 8
U2 24
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
EI 1558-0571
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD APR
PY 2016
VL 13
IS 4
BP 475
EP 479
DI 10.1109/LGRS.2015.2491643
PG 5
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA DH7YJ
UT WOS:000373009800001
ER
PT J
AU Durden, SL
Tanelli, S
Epp, LW
Jamnejad, V
Long, EM
Perez, RM
Prata, A
AF Durden, Stephen L.
Tanelli, Simone
Epp, Larry W.
Jamnejad, Vahraz
Long, Ezra M.
Perez, Raul M.
Prata, Aluizio, Jr.
TI System Design and Subsystem Technology for a Future Spaceborne Cloud
Radar
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Clouds; Dragonian antenna; meteorological radar; precipitation; radar;
radar remote sensing; weather
ID PROFILING RADAR; W-BAND; PERFORMANCE; PROPOSAL; SURFACE
AB The 2007 Decadal Survey for the National Aeronautics and Space Administration recommended an Aerosol/Cloud/Ecosystems (ACE) mission with a new advanced cloud profiling radar. In this letter, we describe ACERAD, a radar design that could meet the goals for the ACE mission. ACERAD has 35 GHz (Ka-band) and 94 GHz (W-band) channels. It would scan at Ka-band and be nadir looking at W-band. The scanning antenna geometry is a classical Dragonian illuminated by a feed array; a reduced-size prototype of the antenna has been successfully fabricated and tested. ACERAD also uses a quasi-optical transmission line at W-band for low-loss routing of the signal from the transmitter to the antenna and from the antenna to the receiver. This letter briefly describes the ACERAD instrument design and test results for some of the major technologies needed for ACERAD implementation.
C1 [Durden, Stephen L.; Tanelli, Simone; Epp, Larry W.; Jamnejad, Vahraz; Long, Ezra M.; Perez, Raul M.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Prata, Aluizio, Jr.] Univ So Calif, Los Angeles, CA 90007 USA.
RP Durden, SL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM sdurden@jpl.nasa.gov
FU NASA Earth Science Technology Office; NASA Aerosol/Cloud/Ecosystems
Study Program
FX This work was supported in part by the NASA Earth Science Technology
Office and in part by the NASA Aerosol/Cloud/Ecosystems Study Program.
NR 25
TC 1
Z9 1
U1 5
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
EI 1558-0571
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD APR
PY 2016
VL 13
IS 4
BP 560
EP 564
DI 10.1109/LGRS.2016.2525718
PG 5
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA DH7YJ
UT WOS:000373009800018
ER
PT J
AU Pan, JM
Durand, M
Sandells, M
Lemmetyinen, J
Kim, EJ
Pulliainen, J
Kontu, A
Derksen, C
AF Pan, Jinmei
Durand, Michael
Sandells, Melody
Lemmetyinen, Juha
Kim, Edward J.
Pulliainen, Jouni
Kontu, Anna
Derksen, Chris
TI Differences Between the HUT Snow Emission Model and MEMLS and Their
Effects on Brightness Temperature Simulation
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Model comparison; passive microwave remote sensing; snow
ID RADIATIVE-TRANSFER THEORY; QUASI-CRYSTALLINE APPROXIMATION; WATER
EQUIVALENT RETRIEVAL; MICROWAVE EMISSION; DRY SNOW; LAYERED SNOWPACKS;
GRAIN-SIZE; MEDIA; SCATTERING; CLASSIFICATION
AB Microwave emission models are a critical component of snow water equivalent retrieval algorithms applied to passive microwave measurements. Several such emission models exist, but their differences need to be systematically compared. This paper compares the basic theories of two models: the multiple-layer Helsinki University of Technology (HUT) model and the microwave emission model of layered snowpacks (MEMLS). By comparing the mathematical formulation side by side, three major differences were identified: 1) by assuming that the scattered intensity is mostly (96%) in the forward direction, the HUT model simplifies the radiative transfer equation in 4p space into two one-flux equations, whereas MEMLS uses a two-flux theory; 2) the HUT scattering coefficient is much larger than the one of MEMLS; and 3) MEMLS considers the trapped radiation inside snow due to internal reflection by a six-flux model, which is not included in HUT. Simulation experiments indicate that the large scattering coefficient of the HUT model compensates for its large forward scattering ratio to some extent, but the effects of one-flux simplification and the trapped radiation still result in different TB simulations between the HUT model and MEMLS. The models were compared with observations of natural snow cover at Sodankyla, Finland; Churchill, Canada; and Colorado, USA. No optimization of the snow grain size was performed. It shows that the HUT model tends to underestimate TB for deep snow. MEMLS with the physically based improved Born approximation performed best among the models, with a bias of -1.4 K and a root-mean-square error of 11.0 K.
C1 [Pan, Jinmei; Durand, Michael] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
[Pan, Jinmei; Durand, Michael] Ohio State Univ, Byrd Polar & Climate Res Ctr, Columbus, OH 43210 USA.
[Sandells, Melody] Univ Reading, Natl Ctr Earth Observat, Reading RG6 6BB, Berks, England.
[Sandells, Melody] Engn & Sci Ltd, Ctr Open Res CORES, Newcastle Upon Tyne NE39 2JA, Tyne & Wear, England.
[Lemmetyinen, Juha; Pulliainen, Jouni; Kontu, Anna] Finish Meteorol Inst, Art Res Ctr, Sodankyla 99600, Finland.
[Kim, Edward J.] NASA, Hydrospher & Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Derksen, Chris] Environm Canada, Div Climate Res, Toronto, ON M3H 5T4, Canada.
[Derksen, Chris] Univ Waterloo, Dept Geog & Environm Management, Waterloo, ON N2L 3G1, Canada.
RP Pan, JM; Durand, M (reprint author), Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.; Pan, JM; Durand, M (reprint author), Ohio State Univ, Byrd Polar & Climate Res Ctr, Columbus, OH 43210 USA.; Sandells, M (reprint author), Univ Reading, Natl Ctr Earth Observat, Reading RG6 6BB, Berks, England.; Sandells, M (reprint author), Engn & Sci Ltd, Ctr Open Res CORES, Newcastle Upon Tyne NE39 2JA, Tyne & Wear, England.; Lemmetyinen, J; Pulliainen, J; Kontu, A (reprint author), Finish Meteorol Inst, Art Res Ctr, Sodankyla 99600, Finland.; Kim, EJ (reprint author), NASA, Hydrospher & Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Derksen, C (reprint author), Environm Canada, Div Climate Res, Toronto, ON M3H 5T4, Canada.; Derksen, C (reprint author), Univ Waterloo, Dept Geog & Environm Management, Waterloo, ON N2L 3G1, Canada.
EM pan.290@osu.edu; durand.8@osu.edu; melody.sandells@coresscience.co.uk;
juha.lemmetyinen@fmi.fi; ed.kim@nasa.gov; jouni.pulliainen@fmi.fi;
anna.kontu@fmi.fi; chris.derksen@ec.gc.ca
RI Kontu, Anna/O-8886-2014
OI Kontu, Anna/0000-0001-6880-6260
FU China Scholarship Council; NASA New Investigator Program [NNX13AB63G];
National Centre for Earth Observation Project [R8/H12/82 NERC]
FX This work was supported in part by the China Scholarship Council
(2012-2016), by the NASA New Investigator Program under Grant
NNX13AB63G, and by the National Centre for Earth Observation Project
(R8/H12/82 NERC).
NR 54
TC 5
Z9 5
U1 2
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD APR
PY 2016
VL 54
IS 4
BP 2001
EP 2019
DI 10.1109/TGRS.2015.2493505
PG 19
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA DH7WF
UT WOS:000373004000011
ER
PT J
AU Le Vine, DM
Abraham, S
Peng, JZ
AF Le Vine, David M.
Abraham, Saji
Peng, Jinzheng
TI Faraday Rotation Correction for the SMAP Radiometer
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Land surface; passive microwave remote sensing; soil moisture
ID 3RD STOKES PARAMETER; L-BAND; ANTENNA PATTERN; MICROWAVE; SPACE;
RETRIEVAL; WATER
AB Faraday rotation is an important issue for remote sensing of parameters such as soil moisture and ocean salinity, which are best done at low microwave frequency (e.g., L-band). Modern instruments such as the radiometer on the Soil Moisture and Ocean Salinity (SMOS) satellite and the Aquarius radiometers include polarimetric radiometer channels specifically to implement a correction for Faraday rotation. This works well over ocean, but it is known that over inhomogeneous scenes, such as a land/water mixture, significant errors can occur. This is a particularly important issue for the newest L-band sensor in space, the radiometer on the Soil Moisture Active Passive (SMAP) satellite, where the goal is remote sensing over land (soil moisture) and where the conical scan induces rapid variation in Faraday rotation. Analysis is presented here of the issues associated with retrieving Faraday rotation using the SMAP geometry and antenna pattern. It is shown that, in addition to scenes with a mixture of land and water, scenes with significant vegetation canopy are also associated with large errors in the retrieved Faraday rotation. Examples from the SMAP radiometer support the analysis.
C1 [Le Vine, David M.; Abraham, Saji; Peng, Jinzheng] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Le Vine, DM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM david.m.levine@nasa.gov
NR 27
TC 1
Z9 1
U1 7
U2 11
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD APR
PY 2016
VL 54
IS 4
BP 2070
EP 2081
DI 10.1109/TGRS.2015.2495168
PG 12
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA DH7WF
UT WOS:000373004000016
ER
PT J
AU Mercer, E
Rungta, N
Gillan, DJ
AF Mercer, Eric
Rungta, Neha
Gillan, Douglas J.
TI Special Issue on Systematic Approaches to Human-Machine Interface:
Improving Resilience, Robustness, and Stability
SO IEEE TRANSACTIONS ON HUMAN-MACHINE SYSTEMS
LA English
DT Editorial Material
ID HUMAN-AUTOMATION INTERACTION; FORMAL VERIFICATION; MODEL CHECKING;
DESIGN; ERROR
C1 [Mercer, Eric] Brigham Young Univ, Provo, UT 84602 USA.
[Rungta, Neha] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Gillan, Douglas J.] N Carolina State Univ, Raleigh, NC 27695 USA.
RP Mercer, E (reprint author), Brigham Young Univ, Provo, UT 84602 USA.
NR 24
TC 0
Z9 0
U1 2
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2168-2291
EI 2168-2305
J9 IEEE T HUM-MACH SYST
JI IEEE T. Hum.-Mach. Syst.
PD APR
PY 2016
VL 46
IS 2
BP 169
EP 173
DI 10.1109/THMS.2016.2516780
PG 5
WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics
SC Computer Science
GA DH5OV
UT WOS:000372841200001
ER
PT J
AU Krall, J
Menzies, T
Davies, M
AF Krall, Joseph
Menzies, Tim
Davies, Misty
TI Learning Mitigations for Pilot Issues When Landing Aircraft (via
Multiobjective Optimization and Multiagent Simulations)
SO IEEE TRANSACTIONS ON HUMAN-MACHINE SYSTEMS
LA English
DT Article
DE Active Learning; cognitive modeling; human factors; multiobjective
optimization
ID DIFFERENTIAL EVOLUTION; ALGORITHM; MODELS
AB We advocate exploring complex models by combining data miners (to find a small set of most critical examples) and of multiobjective optimizers (that focus on those critical examples). An example of such a combination is the GALE optimizer that intelligently explores thousands of scenarios by examining just a few dozen of the most informative examples. GALE-style reasoning enables a very fast, very wide ranging exploration of behaviors, as well as the effects of those behaviors' limitations. This paper applies GALE to the continuous descent approach (CDA) model within the Georgia Tech Work Models that Compute framework. CDA is a model of pilot interactions: with each other and also with the navigation systems critical to safe flight. We show that, using CDA+GALE, it is possible to identify and mitigate factors that make pilots unable to complete all their required tasks in the context of different 1) function allocation strategies, 2) pilot cognitive control strategies, and 3) operational contexts that impact and safe aircraft operation. We also show that other optimization methods can be so slow to run that, without GALE, it might be impractical to find those mitigations.
C1 [Krall, Joseph] LoadIQ, Reno, NV 89501 USA.
[Menzies, Tim] N Carolina State Univ, Dept Comp Sci, Raleigh, NC 27695 USA.
[Davies, Misty] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
RP Krall, J (reprint author), LoadIQ, Reno, NV 89501 USA.; Menzies, T (reprint author), N Carolina State Univ, Dept Comp Sci, Raleigh, NC 27695 USA.; Davies, M (reprint author), NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
EM kralljoe@gmail.com; tim.menzies@gmail.com; misty.d.davies@nasa.gov
NR 34
TC 1
Z9 1
U1 3
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2168-2291
EI 2168-2305
J9 IEEE T HUM-MACH SYST
JI IEEE T. Hum.-Mach. Syst.
PD APR
PY 2016
VL 46
IS 2
BP 221
EP 230
DI 10.1109/THMS.2015.2509980
PG 10
WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics
SC Computer Science
GA DH5OV
UT WOS:000372841200006
ER
PT J
AU Combefis, S
Giannakopoulou, D
Pecheur, C
AF Combefis, Sebastien
Giannakopoulou, Dimitra
Pecheur, Charles
TI Automatic Detection of Potential Automation Surprises for ADEPT Models
SO IEEE TRANSACTIONS ON HUMAN-MACHINE SYSTEMS
LA English
DT Article
DE ADEPT toolset; formal methods; human factors; human-machine interaction
ID ERRONEOUS HUMAN-BEHAVIOR; FORMAL VERIFICATION; CHECKING; SAFETY;
KNOWLEDGE; SYSTEMS
AB This paper describes how to automatically detect potential automation surprises in interactive systems, within a rapid automation interface design tool named ADEPT. The proposed analysis method in this paper is based on a conformance relation, called full-control, between the model of the actual system and a mental model of it, that is, its behavior as perceived by the operator. The method can, among other things, automatically generate a so-called minimal full-control mental model for a given system. Systems are well designed if they can be described by relatively simple mental models for their operators, which can be assessed with the minimal full-control mental model generation algorithms. During the generation, potential automation surprises are detected and highlighted with execution examples that may lead to confusion. The analysis methods are based on an enriched version of labeled transition systems to describe the system and mental models. In order to be able to integrate the analysis method within ADEPT, a semantics for ADEPT models makes it possible to translate them into enriched LTSs. The proposed translation is automated for a specified class of ADEPT models that are characterized and defined in this paper. A case study demonstrates the proposed analysis framework and informs how the integration with ADEPT can be improved.
C1 [Combefis, Sebastien] Ecole Cent Arts & Metiers, B-1200 Brussels, Belgium.
[Giannakopoulou, Dimitra] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Pecheur, Charles] Catholic Univ Louvain, Elect & Appl Math Inst, ICT, B-1348 Louvain La Neuve, Belgium.
RP Combefis, S (reprint author), Ecole Cent Arts & Metiers, B-1200 Brussels, Belgium.; Giannakopoulou, D (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA.; Pecheur, C (reprint author), Catholic Univ Louvain, Elect & Appl Math Inst, ICT, B-1348 Louvain La Neuve, Belgium.
EM s.combefis@ecam.be; dimitra.giannakopoulou@nasa.gov;
charles.pecheur@uclouvain.be
NR 38
TC 0
Z9 0
U1 1
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2168-2291
EI 2168-2305
J9 IEEE T HUM-MACH SYST
JI IEEE T. Hum.-Mach. Syst.
PD APR
PY 2016
VL 46
IS 2
BP 267
EP 278
DI 10.1109/THMS.2015.2424851
PG 12
WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics
SC Computer Science
GA DH5OV
UT WOS:000372841200010
ER
PT J
AU Jin, ZH
Sun, MG
AF Jin, Zhonghai
Sun, Moguo
TI An Initial Study on Climate Change Fingerprinting Using the Reflected
Solar Spectra
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Variability; Cloud radiative effects; Interannual variability;
Variational analysis; Radiative transfer; Mathematical and statistical
techniques; Physical Meteorology and Climatology
ID INFRARED-SPECTRA; MODELS; ATTRIBUTION
AB Attribution of averaged spectral variation over large spatial and temporal scales to different climate variables is central to climate change fingerprinting. Using 10 years of satellite data for simulation, the authors generate a group of observation-based spectral fingerprints and a time series of monthly mean reflectance spectra over the ocean in five large latitude regions and globally. Next, these fingerprints and the interannual variation spectra are used to retrieve the interannual changes in the relevant climate variables to test the concept of using the spectral fingerprinting approach for climate change attribution. Comparing the fingerprinting retrieval of climate variable change to the actual underlying variable change, the RMS differences between the two are less than twice as large as the monthly variability for all variables in all regions. Instances where larger errors are observed correspond to those variables with large nonlinear radiative response, such as the cloud optical depth and the ice particle size. Using the linear fingerprinting approach and accounting for the nonlinear radiative error in fingerprints results in significantly higher retrieval accuracy; the RMS errors are reduced to less than the monthly variability for nearly all variables, indicating the profound impact of the nonlinear error on fingerprinting retrieval. Another important finding is that if the cloud fraction is known a priori, the retrieval accuracy in cloud optical depth would be improved substantially. Moreover, a better retrieval for the water vapor amount and aerosol optical depth can be achieved from the clear-sky data only. The test results demonstrate that climate change fingerprinting based on reflected solar benchmark spectra is possible.
C1 [Jin, Zhonghai; Sun, Moguo] NASA, Langley Res Ctr, Sci Syst & Applicat & Climate Sci Branch, Hampton, VA 23681 USA.
RP Jin, ZH (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM zhonghai.jin@nasa.gov
FU Radiation Sciences Program; CLARREO project of NASA's Earth Science
Division
FX We thank the NASA CERES group for the SSF data, Dr. Sky Yang and Dr.
Shuntai Zhou for the ozone data, and Amber Richards and Rosemary Baize
for help in editing. This research is supported by the Radiation
Sciences Program and the CLARREO project of NASA's Earth Science
Division.
NR 25
TC 2
Z9 2
U1 3
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD APR
PY 2016
VL 29
IS 8
BP 2781
EP 2796
DI 10.1175/JCLI-D-15-0297.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DI2WW
UT WOS:000373360900001
ER
PT J
AU Viterbo, F
von Hardenberg, J
Provenzale, A
Molini, L
Parodi, A
Sy, OO
Tanelli, S
AF Viterbo, Francesca
von Hardenberg, Jost
Provenzale, Antonello
Molini, Luca
Parodi, Antonio
Sy, Ousmane O.
Tanelli, Simone
TI High-Resolution Simulations of the 2010 Pakistan Flood Event:
Sensitivity to Parameterizations and Initialization Time
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Complex terrain; Atm/Ocean Structure/ Phenomena; Models and modeling;
Nonhydrostatic models; Observational techniques and algorithms;
Precipitation; Satellite observations; Convective parameterization;
Geographic location/entity; Cloud microphysics; Physical Meteorology and
Climatology
ID OBJECT-BASED VERIFICATION; CONVECTIVE PARAMETERIZATION; PRECIPITATION
FORECASTS; HORIZONTAL RESOLUTION; TIBETAN PLATEAU; WRF SIMULATION; PART
II; RAINFALL; MODEL; MICROPHYSICS
AB Estimating the risk of flood-generating precipitation events in high-mountain regions with complex orography is a difficult but crucial task. Quantitative precipitation forecasts (QPFs) at fine resolution are an essential ingredient to address this issue. Along these lines, the ability of the Weather Research and Forecasting (WRF) Model, operated at 3.5-km grid spacing, to reproduce the extreme meteorological event that led to the 2010 Pakistan flood and produced heavy monsoonal rain in the Indus basin is explored. The model results are compared with Tropical Rainfall Measuring Mission (TRMM) rainfall estimates, the available ground measurements, and radar observations from the CloudSat mission. In particular, the sensitivity of the WRF simulations to the use of different convective closures (explicit and Kain-Fritsch) and microphysical parameterizations (WRF single-moment 6-class microphysics scheme and Thompson) is analyzed. The impact of using different initial conditions, associated with a different initialization day, is also examined. The use of the new-generation Distributed Simulation and Stimulation System NASA Earth Observing System Simulators Suite radar simulator allows a more accurate and extensive representation of the mesoscale processes and of the interaction with the complex orography. The results reported here indicate that the quality of the large-scale initial conditions is a prominent factor affecting the possibility of retrieving a realistic representation of this event when using a nonhydrostatic regional model.
C1 [Viterbo, Francesca; von Hardenberg, Jost] CNR, Inst Atmospher Sci & Climate, Corso Fiume 4, I-10133 Turin, Italy.
[Viterbo, Francesca] Univ Genoa, Genoa, Italy.
[Provenzale, Antonello] CNR, Inst Geosci & Earth Resources, Pisa, Italy.
[Molini, Luca; Parodi, Antonio] CIMA Fdn, Savona, Italy.
[Sy, Ousmane O.; Tanelli, Simone] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Viterbo, F (reprint author), CNR, Inst Atmospher Sci & Climate, Corso Fiume 4, I-10133 Turin, Italy.
EM f.viterbo@isac.cnr.it
FU Italian Ministry for Education, University and Research; National
Aeronautics and Space Administration; SuperMUC Petascale System of the
LRZ Supercomputing Centre, Garching, Germany [pr45de]
FX This work was supported by the PNR 2011-13 Project of National Interest
"NextData'' and by the 2010-11 Project of National Interest "Innovative
methods for water resources management and risk assessment under
uncertainty" of the Italian Ministry for Education, University and
Research. The work of Dr. Tanelli and Dr. Sy was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. This
work was carried out in support of the CloudSat and GPM missions. The
authors are also grateful to the Pakistan Meteorological Department for
the provision of the daily rainfall rain gauges data, as well as to the
Editor and the four anonymous reviewers for their constructive comments
on the early version of the manuscript. The numerical simulations were
performed on the SuperMUC Petascale System of the LRZ Supercomputing
Centre, Garching, Germany. Project-ID: pr45de.
NR 60
TC 0
Z9 0
U1 8
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD APR
PY 2016
VL 17
IS 4
BP 1147
EP 1167
DI 10.1175/JHM-D-15-0098.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DI2GL
UT WOS:000373313600001
ER
PT J
AU Gonzalez, AO
Slocum, CJ
Taft, RK
Schubert, WH
AF Gonzalez, Alex O.
Slocum, Christopher J.
Taft, Richard K.
Schubert, Wayne H.
TI Dynamics of the ITCZ Boundary Layer
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Models and modeling; Atm/Ocean Structure/ Phenomena; Boundary layer;
Circulation/ Dynamics; Geographic location/entity; Nonlinear models;
Dynamics; Intertropical convergence zone
ID INTERTROPICAL CONVERGENCE ZONE; EASTERN EQUATORIAL PACIFIC; SEA-SURFACE
TEMPERATURE; TROPICAL PACIFIC; LOW-LATITUDE; OCEAN MODEL; CONVECTION;
ATMOSPHERE; GRADIENTS; HURRICANE
AB This paper presents high-resolution numerical solutions of a nonlinear zonally symmetric slab model of the intertropical convergence zone (ITCZ) boundary layer. The boundary layer zonal and meridional flows are forced by a specified pressure field, which can also be interpreted as a specified geostrophically balanced zonal wind field u(g)(y). One narrow on-equatorial peak in boundary layer pumping is produced when the forcing is easterly geostrophic flow along the equator and two narrow peaks in boundary layer pumping are produced on opposite sides of the equator (a double ITCZ) when the forcing is westerly geostrophic flow along the equator. In the case when easterlies are surrounding a westerly wind burst, once again a double ITCZ is produced, but the ITCZs have significantly more intense boundary layer pumping than the case of only westerly geostrophic flow. A comparison of the numerical solutions to those of classical Ekman theory suggests that the meridional advection term upsilon( partial differential upsilon/ partial differential y) plays a vital role in strengthening and narrowing boundary layer pumping regions while weakening and broadening boundary layer suction regions.
C1 [Gonzalez, Alex O.; Slocum, Christopher J.; Taft, Richard K.; Schubert, Wayne H.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Gonzalez, Alex O.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Gonzalez, Alex O.] CALTECH, Jet Prop Lab, MS 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Gonzalez, AO (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.; Gonzalez, AO (reprint author), CALTECH, Jet Prop Lab, MS 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM alex.o.gonzalez@jpl.nasa.gov
FU National Science Foundation [AGS-1250966]; Science and Technology Center
for Multi-Scale Modeling of Atmospheric Processes [ATM-0425247]
FX We thank Paul Ciesielski, Thomas Birner, Eric Maloney, and Donald Estep
for their insightful discussions. We would like to acknowledge the
reviewers, Adam Sobel and David Raymond, for their constructive comments
on the manuscript. This research has been supported by the National
Science Foundation under Grant AGS-1250966 and under the Science and
Technology Center for Multi-Scale Modeling of Atmospheric Processes,
managed by Colorado State University through Cooperative Agreement
ATM-0425247.
NR 46
TC 0
Z9 0
U1 1
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD APR
PY 2016
VL 73
IS 4
BP 1577
EP 1592
DI 10.1175/JAS-D-15-0298.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DG9LF
UT WOS:000372403800001
ER
PT J
AU Morton, DC
AF Morton, Douglas C.
TI FOREST CARBON FLUXES A satellite perspective
SO NATURE CLIMATE CHANGE
LA English
DT Editorial Material
ID TROPICAL REGIONS; EMISSIONS; DEFORESTATION; MAP; STOCKS
AB Reducing deforestation and forest degradation offers a quick win for climate mitigation. Using satellite data we are now able to better constrain pantropical estimates of forest loss, reshaping our understanding of the annual to decadal variability in land sources and sinks in the global carbon cycle.
C1 [Morton, Douglas C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Morton, DC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM douglas.morton@nasa.gov
RI Morton, Douglas/D-5044-2012
NR 15
TC 3
Z9 3
U1 7
U2 23
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
EI 1758-6798
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD APR
PY 2016
VL 6
IS 4
BP 346
EP 348
PG 4
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DH8QI
UT WOS:000373060000008
ER
PT J
AU Marvel, K
Schmidt, GA
Miller, RL
Nazarenko, LS
AF Marvel, Kate
Schmidt, Gavin A.
Miller, Ron L.
Nazarenko, Larissa S.
TI Implications for climate sensitivity from the response to individual
forcings
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID SYSTEM PROPERTIES; GISS MODELE2; SIMULATIONS; CONSTRAINTS
AB Climate sensitivity to doubled CO2 is a widely used metric for the large-scale response to external forcing. Climate models predict a wide range for two commonly used definitions: the transient climate response (TCR: the warming after 70 years of CO2 concentrations that rise at 1% per year), and the equilibrium climate sensitivity (ECS: the equilibrium temperature change following a doubling of CO2 concentrations). Many observational data sets have been used to constrain these values, including temperature trends over the recent past(1-6), inferences from palaeoclimate(7,8) and process-based constraints from the modern satellite era(9,10). However, as the IPCC recently reported(11), different classes of observational constraints produce somewhat incongruent ranges. Here we show that climate sensitivity estimates derived from recent observations must account for the efficacy of each forcing active during the historical period. When we use single-forcing experiments to estimate these efficacies and calculate climate sensitivity from the observed twentieth-century warming, our estimates of both TCR and ECS are revised upwards compared to previous studies, improving the consistency with independent constraints.
C1 [Marvel, Kate; Miller, Ron L.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
[Marvel, Kate; Schmidt, Gavin A.; Miller, Ron L.; Nazarenko, Larissa S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Nazarenko, Larissa S.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
RP Marvel, K; Miller, RL (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.; Marvel, K; Schmidt, GA; Miller, RL (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM kate.marvel@nasa.gov; gavin.a.schmidt@nasa.gov; ron.l.miller@nasa.gov
RI Miller, Ron/E-1902-2012;
OI Schmidt, Gavin/0000-0002-2258-0486
FU NASA Modeling, Analysis and Prediction Program; NASA High-End Computing
(HEC) Program through the NASA Center for Climate Simulation (NCCS) at
Goddard Space Flight Center
FX Climate modelling at GISS is supported by the NASA Modeling, Analysis
and Prediction Program and resources supporting this work were provided
by the NASA High-End Computing (HEC) Program through the NASA Center for
Climate Simulation (NCCS) at Goddard Space Flight Center. The authors
thank D. McNeall and E. Hawkins for advice on figures, and E. Hawkins,
J. Gregory, M. Webb, K. Taylor and R. Pincus for helpful discussions.
NR 30
TC 13
Z9 13
U1 9
U2 18
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
EI 1758-6798
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD APR
PY 2016
VL 6
IS 4
BP 386
EP 389
DI 10.1038/NCLIMATE2888
PG 4
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DH8QI
UT WOS:000373060000015
ER
PT J
AU Taylor, LL
Quirk, J
Thorley, RMS
Kharecha, PA
Hansen, J
Ridgwell, A
Lomas, MR
Banwart, SA
Beerling, DJ
AF Taylor, Lyla L.
Quirk, Joe
Thorley, Rachel M. S.
Kharecha, Pushker A.
Hansen, James
Ridgwell, Andy
Lomas, Mark R.
Banwart, Steve A.
Beerling, David J.
TI Enhanced weathering strategies for stabilizing climate and averting
ocean acidification
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID EARTH SYSTEM MODELS; CARBON-DIOXIDE; FUTURE CLIMATE; CO2; CYCLE; TIME;
SENSITIVITY; CHEMISTRY; RESPONSES
AB Chemical breakdown of rocks, weathering, is an important but very slow part of the carbon cycle that ultimately leads to CO2 being locked up in carbonates on the ocean floor. Artificial acceleration of this carbon sink via distribution of pulverized silicate rocks across terrestrial landscapesmay help offset anthropogenic CO2 emissions(1-5). We show that idealized enhanced weathering scenarios over less than a third of tropical land could cause significant drawdown of atmospheric CO2 and ameliorate ocean acidification by 2100. Global carbon cycle modelling(6-8) driven by ensemble Representative Concentration Pathway (RCP) projections of twenty-first-century climate change (RCP8.5, business-as-usual; RCP4.5, medium-level mitigation)(9,10) indicates that enhanced weathering could lower atmospheric CO2 by 30-300 ppm by 2100, depending mainly on silicate rock application rate (1 kg or 5 kg m(-2) yr(-1)) and composition. At the higher application rate, end-of-century ocean acidification is reversed under RCP4.5 and reduced by about two-thirds under RCP8.5. Additionally, surface ocean aragonite saturation state, a key control on coral calcification rates, is maintained above 3.5 throughout the low latitudes, thereby helping maintain the viability of tropical coral reef ecosystems(11-14). However, we highlight major issues of cost, social acceptability, and potential unanticipated consequences that will limit utilization and emphasize the need for urgent efforts to phase down fossil fuel emissions(15).
C1 [Taylor, Lyla L.; Quirk, Joe; Thorley, Rachel M. S.; Beerling, David J.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England.
[Kharecha, Pushker A.; Hansen, James] Columbia Univ, Earth Inst, 475 Riverside Dr, New York, NY 10027 USA.
[Kharecha, Pushker A.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Ridgwell, Andy] Univ Bristol, Dept Geog Sci, Bristol BS8 1SS, Avon, England.
[Ridgwell, Andy] Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA.
[Lomas, Mark R.] Univ Sheffield, Dept Math, Sheffield S10 2TN, S Yorkshire, England.
[Banwart, Steve A.] Univ Sheffield, Kroto Res Inst, North Campus, Sheffield S3 7HQ, S Yorkshire, England.
RP Beerling, DJ (reprint author), Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England.
EM d.j.beerling@sheffield.ac.uk
OI Quirk, Joe/0000-0002-0625-8323
FU ERC [32998]
FX We thank Y. Godderis and P. Renforth for helpful comments on the
manuscript, T. Elliot for earlier discussions, and gratefully
acknowledge funding through an ERC Advanced grant to D.J.B. (CDREG,
32998). We acknowledge the World Climate Research Programme's Working
Group on Coupled Modelling, which is responsible for CMIP, and we thank
the climate modelling groups (Supplementary Table 1) for producing and
making available their model output. For CMIP the US Department of
Energy's Program for Climate Model Diagnosis and Intercomparison
provides coordinating support and led development of software
infrastructure in partnership with the Global Organization for Earth
System Science Portals.
NR 53
TC 5
Z9 5
U1 30
U2 68
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
EI 1758-6798
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD APR
PY 2016
VL 6
IS 4
BP 402
EP +
DI 10.1038/NCLIMATE2882
PG 7
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DH8QI
UT WOS:000373060000019
ER
PT J
AU Lim, YK
Kim, HD
AF Lim, Young-Kwon
Kim, Hae-Dong
TI Comparison of the impact of the Arctic Oscillation and Eurasian
teleconnection on interannual variation in East Asian winter
temperatures and monsoon
SO THEORETICAL AND APPLIED CLIMATOLOGY
LA English
DT Article
ID ATMOSPHERIC CIRCULATION; GEOPOTENTIAL HEIGHT; SEA-ICE; PATTERNS;
NORTHERN; CLIMATE; MODES; VARIABILITY; ANOMALIES; INDEX
AB The large-scale impacts of the Arctic Oscillation (AO) and the Eurasian teleconnection (EU) on the East Asian winter climate are compared for the past 34 winters, focusing on (1) interannual monthly to seasonal temperature variability, (2) East Asian winter monsoon (EAWM), and (3) the Siberian high (SH) and cold surge. Regression analysis reveals warming by AO and cooling by EU over mid-latitude East Asia during their positive phase and vice versa (i.e., warm phase: +AO, -EU; cold phase: -AO, +EU). The EU impact was found to be comparable to the AO impact. For example, warm (cold) months during the warm (cold) AO phase are found clearly when the AO is in the same warm (cold) EU phase. No significant correlation was found between East Asian temperature and the AO when the warm (cold) AO coincided with the cold (warm) EU. The well-known relationship of strong (weak) SH during the cold (warm) AO phase was observed significantly more often when the AO was in the same cold (warm) EU phase. Also, the indices of EAWM, cold surge, and SH were more highly correlated with the EU than with the AO. The advective temperature change and associated circulation demonstrate that the large-scale field including the SH over the mid-latitude Asian inland is better represented by the EU, influencing the East Asian climate. These results suggest that the impact of EU should be considered more important than previously thought for a better understanding of East Asian winter temperature and monsoon variability.
C1 [Lim, Young-Kwon] NASA, Goddard Space Flight Ctr, GESTAR, IM Syst Grp, Greenbelt, MD USA.
[Kim, Hae-Dong] Keimyung Univ, Coll Environm, Daegu, South Korea.
RP Kim, HD (reprint author), Keimyung Univ, Coll Environm, Daegu, South Korea.
EM Young-Kwon.Lim@nasa.gov; khd@kmu.ac.kr
FU Keimyung University
FX This research was supported by the Scholar Research Grant of Keimyung
University in 2013.
NR 36
TC 3
Z9 3
U1 4
U2 11
PU SPRINGER WIEN
PI WIEN
PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA
SN 0177-798X
EI 1434-4483
J9 THEOR APPL CLIMATOL
JI Theor. Appl. Climatol.
PD APR
PY 2016
VL 124
IS 1-2
BP 267
EP 279
DI 10.1007/s00704-015-1418-x
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DH9VH
UT WOS:000373143600020
ER
PT J
AU Srivastava, PK
Han, DW
Islam, T
Petropoulos, GP
Gupta, M
Dai, Q
AF Srivastava, Prashant K.
Han, Dawei
Islam, Tanvir
Petropoulos, George P.
Gupta, Manika
Dai, Qiang
TI Seasonal evaluation of evapotranspiration fluxes from MODIS satellite
and mesoscale model downscaled global reanalysis datasets
SO THEORETICAL AND APPLIED CLIMATOLOGY
LA English
DT Article
ID SMOS SOIL-MOISTURE; CROP EVAPOTRANSPIRATION; INCREMENTAL APPROACH; WRF
MODEL; VALIDATION; PERFORMANCE; ALGORITHM; PRODUCTS; SURFACES; FUTURE
AB Reference evapotranspiration (ETo) is an important variable in hydrological modeling, which is not always available, especially for ungauged catchments. Satellite data, such as those available from the MODerate Resolution Imaging Spectroradiometer (MODIS), and global datasets via the European Centre for Medium Range Weather Forecasts (ECMWF) reanalysis (ERA) interim and National Centers for Environmental Prediction (NCEP) reanalysis are important sources of information for ETo. This study explored the seasonal performances of MODIS (MOD16) and Weather Research and Forecasting (WRF) model downscaled global reanalysis datasets, such as ERA interim and NCEP-derived ETo, against ground-based datasets. Overall, on the basis of the statistical metrics computed, ETo derived from ERA interim and MODIS were more accurate in comparison to the estimates from NCEP for all the seasons. The pooled datasets also revealed a similar performance to the seasonal assessment with higher agreement for the ERA interim (r = 0.96, RMSE = 2.76 mm/8 days; bias = 0.24 mm/8 days), followed by MODIS (r = 0.95, RMSE = 7.66 mm/8 days; bias = -7.17 mm/8 days) and NCEP (r = 0.76, RMSE = 11.81 mm/8 days; bias = -10.20 mm/8 days). The only limitation with downscaling ERA interim reanalysis datasets using WRF is that it is time-consuming in contrast to the readily available MODIS operational product for use in mesoscale studies and practical applications.
C1 [Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Hydrol Sci, Greenbelt, MD 20771 USA.
[Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Srivastava, Prashant K.; Han, Dawei; Islam, Tanvir; Dai, Qiang] Univ Bristol, Dept Civil Engn, Bristol, Avon, England.
[Islam, Tanvir] NOAA, NESDIS, Ctr Satellite Applicat & Res, College Pk, MD 20740 USA.
[Islam, Tanvir] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Petropoulos, George P.] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3DB, Dyfed, Wales.
[Gupta, Manika] IIT, Dept Civil Engn, Water Resources, Delhi 110016, India.
RP Srivastava, PK (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci, Greenbelt, MD 20771 USA.; Srivastava, PK (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.; Srivastava, PK (reprint author), Univ Bristol, Dept Civil Engn, Bristol, Avon, England.
EM prashant.k.srivastava@nasa.gov
RI Petropoulos, George/F-2384-2013;
OI Petropoulos, George/0000-0003-1442-1423; Islam,
Tanvir/0000-0003-2429-3074
FU Commonwealth Scholarship Commission; British Council, UK; Ministry of
Human Resource Development, Government of India
FX The authors would like to thank the Commonwealth Scholarship Commission,
British Council, UK and the Ministry of Human Resource Development,
Government of India for providing the necessary support and funding for
this research. The authors would like to acknowledge the British
Atmospheric Data Centre, UK for providing the ground datasets. The
author also acknowledges the Advanced Computing Research Centre at
University of Bristol for providing the access to supercomputer facility
(The Blue Crystal) for some of the analysis. Dr. Petropoulos's
contribution was supported by the European Commission Marie Curie
Re-Integration Grant "TRANSFORM-EO" project. Authors would also like to
thank Gareth Ireland for the language proof reading of the manuscript.
The views expressed here are those of the authors solely and do not
constitute a statement of policy, decision, or position on behalf of
NOAA/NASA or the authors' affiliated institutions.
NR 52
TC 5
Z9 5
U1 6
U2 12
PU SPRINGER WIEN
PI WIEN
PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA
SN 0177-798X
EI 1434-4483
J9 THEOR APPL CLIMATOL
JI Theor. Appl. Climatol.
PD APR
PY 2016
VL 124
IS 1-2
BP 461
EP 473
DI 10.1007/s00704-015-1430-1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DH9VH
UT WOS:000373143600035
ER
PT J
AU De-Bashan, LE
Mayali, X
Bebout, BM
Weber, PK
Detweiler, AM
Hernandez, JP
Prufert-Bebout, L
Bashan, Y
AF de-Bashan, Luz E.
Mayali, Xavier
Bebout, Brad M.
Weber, Peter K.
Detweiler, Angela M.
Hernandez, Juan-Pablo
Prufert-Bebout, Leslie
Bashan, Yoav
TI Establishment of stable synthetic mutualism without co-evolution between
microalgae and bacteria demonstrated by mutual transfer of metabolites
(NanoSIMS isotopic imaging) and persistent physical association
(Fluorescent in situ hybridization)
SO ALGAL RESEARCH-BIOMASS BIOFUELS AND BIOPRODUCTS
LA English
DT Article
DE Microalgae; NanoSIMS; Plant growth-promoting bacteria; Synthetic
mutualism
ID GROWTH-PROMOTING BACTERIUM; TARGETED OLIGONUCLEOTIDE PROBES; MICROBIAL
CELL-FACTORIES; CHLORELLA-VULGARIS; AZOSPIRILLUM-BRASILENSE;
PLANT-GROWTH; ALGINATE BEADS; WASTE-WATER; HETEROTROPHIC CONDITIONS;
ENHANCED ACCUMULATION
AB The demonstration of a mutualistic interaction requires evidence of benefits for both partners as well as stability of the association over multiple generations. A synthetic mutualism between the freshwater microalga Chlorella sorokiniana and the soil-derived plant growth-promoting bacterium (PGPB) Azospirillum brasilense was created when both microorganisms were co-immobilized in alginate beads. Using stable isotope enrichment experiments followed by high-resolution secondary ion mass spectrometry (SIMS) imaging of single cells, we demonstrated transfer of carbon and nitrogen compounds between the two partners. Further, using fluorescent in situ hybridization (FISH), mechanical disruption and scanning electron microscopy, we demonstrated the stability of their physical association for a period of 10 days after the aggregated cells were released from the beads. The bacteria significantly enhanced the growth of the microalgae while the microalgae supported growth of the bacteria in a medium where it could not otherwise grow. We propose that this microalga-bacterium association is a true synthetic mutualism independent of co-evolution. (C) 2016 Elsevier B.V. All rights reserved.
C1 [de-Bashan, Luz E.; Hernandez, Juan-Pablo; Bashan, Yoav] Bashan Inst Sci, 1730 Post Oak Court, Auburn, AL 36830 USA.
[de-Bashan, Luz E.; Bashan, Yoav] Auburn Univ, Dept Entomol & Plant Pathol, 301 Funchess Hall, Auburn, AL 36849 USA.
[de-Bashan, Luz E.; Hernandez, Juan-Pablo] Northwestern Ctr Biol Res CIBNOR, Environm Microbiol Grp, Calle IPN 195, La Paz 23096, Bcs, Bolivia.
[Mayali, Xavier; Weber, Peter K.] Lawrence Livermore Natl Lab, Nucl & Chem Sci Div, Livermore, CA 94551 USA.
[Bebout, Brad M.; Detweiler, Angela M.; Prufert-Bebout, Leslie] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Detweiler, Angela M.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
RP Bashan, Y (reprint author), Bashan Inst Sci, 1730 Post Oak Court, Auburn, AL 36830 USA.
EM ybb0001@auburn.edu
OI Hernandez, Juan/0000-0003-1175-0109
FU Consejo Nacional de Ciencia y Tecnologia of Mexico (CONACYT-Basic
Science) [164548]; Bashan Foundation, USA; NASA's Exobiology Program
NASA; LLNL by the DOE-OBER [SCW1039]; US Department of Energy at the
Lawrence Livermore National Laboratory [DE-AC52-07NA27344]
FX Funding was provided in parts by: Consejo Nacional de Ciencia y
Tecnologia of Mexico (CONACYT-Basic Science-2009, grant 164548), by The
Bashan Foundation, USA, by grants from NASA's Exobiology Program NASA to
BMB and at LLNL by the DOE-OBER-funded Biofuels Science Focus Area Grant
SCW1039. We thank Christina Ramon at LLNL for the assistance with SEM
analyses. At CIBNOR, we thank Edgar Amavizca and Ariel Cruz for the
technical assistance in scanning electron microscopy and Paulina Adams
for the general technical assistance. Work at LLNL was performed under
the auspices of the US Department of Energy at the Lawrence Livermore
National Laboratory under Contract DE-AC52-07NA27344. This is
contribution 2015-007 from the Bashan Institute of Science, USA.
NR 64
TC 5
Z9 5
U1 15
U2 38
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 2211-9264
J9 ALGAL RES
JI Algal Res.
PD APR
PY 2016
VL 15
BP 179
EP 186
DI 10.1016/j.algal.2016.02.019
PG 8
WC Biotechnology & Applied Microbiology
SC Biotechnology & Applied Microbiology
GA DH0DK
UT WOS:000372452500021
ER
PT J
AU Schoorlemmer, H
Belov, K
Romero-Wolf, A
Garcia-Fernandez, D
Bugaev, V
Wissel, SA
Allison, P
Alvarez-Muniz, J
Barwick, SW
Beatty, JJ
Besson, DZ
Binns, WR
Carvalho, WR
Chen, C
Chen, P
Clem, JM
Connolly, A
Dowkontt, PF
DuVernois, MA
Field, RC
Goldstein, D
Gorham, PW
Hast, C
Huegen, T
Heber, CL
Hoover, S
Israel, MH
Javaid, A
Kowalski, J
Lam, J
Learned, JG
Link, JT
Lusczek, E
Matsuno, S
Mercurio, BC
Miki, C
Miocinovic, P
Mulrey, K
Nam, J
Naudet, CJ
Ng, J
Nichol, RJ
Palladino, K
Rauch, BF
Roberts, J
Reil, K
Rotter, B
Rosen, M
Ruckman, L
Saltzberg, D
Seckel, D
Urdaneta, D
Varner, GS
Vieregg, AG
Walz, D
Wu, F
Zas, E
AF Schoorlemmer, H.
Belov, K.
Romero-Wolf, A.
Garcia-Fernandez, D.
Bugaev, V.
Wissel, S. A.
Allison, P.
Alvarez-Muniz, J.
Barwick, S. W.
Beatty, J. J.
Besson, D. Z.
Binns, W. R.
Carvalho, W. R., Jr.
Chen, C.
Chen, P.
Clem, J. M.
Connolly, A.
Dowkontt, P. F.
DuVernois, M. A.
Field, R. C.
Goldstein, D.
Gorham, P. W.
Hast, C.
Huegen, T.
Heber, C. L.
Hoover, S.
Israel, M. H.
Javaid, A.
Kowalski, J.
Lam, J.
Learned, J. G.
Link, J. T.
Lusczek, E.
Matsuno, S.
Mercurio, B. C.
Miki, C.
Miocinovic, P.
Mulrey, K.
Nam, J.
Naudet, C. J.
Ng, J.
Nichol, R. J.
Palladino, K.
Rauch, B. F.
Roberts, J.
Reil, K.
Rotter, B.
Rosen, M.
Ruckman, L.
Saltzberg, D.
Seckel, D.
Urdaneta, D.
Varner, G. S.
Vieregg, A. G.
Walz, D.
Wu, F.
Zas, E.
TI Energy and flux measurements of ultra-high energy cosmic rays observed
during the first ANITA flight
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Cosmic rays; Air shower; Radio detection
ID TELESCOPE ARRAY EXPERIMENT; INDUCED AIR-SHOWERS; RADIO-EMISSION; COREAS
SIMULATIONS; ATMOSPHERIC SHOWERS; LOPES MEASUREMENTS; REAS 3.11;
DETECTOR; SURFACE; PULSES
AB The first flight of the Antarctic Impulsive Transient Antenna (ANITA) experiment recorded 16 radio signals that were emitted by cosmic-ray induced air showers. The dominant contribution to the radiation comes from the deflection of positrons and electrons in the geomagnetic field, which is beamed in the direction of motion of the air shower. For 14 of these events, this radiation is reflected from the ice and subsequently detected by the ANITA experiment at a flight altitude of similar to 36 km. In this paper, we estimate the energy of the 14 individual events and find that the mean energy of the cosmic-ray sample is 2.9 x 10(18) eV, which is significantly lower than the previous estimate. By simulating the ANITA flight, we calculate its exposure for ultra-high energy cosmic rays. We estimate for the first time the cosmic-ray flux derived only from radio observations and find agreement with measurements performed at other observatories. In addition, we find that the ANITA data set is consistent with Monte Carlo simulations for the total number of observed events and with, the properties of those events. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Schoorlemmer, H.; DuVernois, M. A.; Gorham, P. W.; Heber, C. L.; Kowalski, J.; Learned, J. G.; Lusczek, E.; Matsuno, S.; Miki, C.; Miocinovic, P.; Nam, J.; Roberts, J.; Rotter, B.; Rosen, M.; Ruckman, L.; Varner, G. S.] Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Schoorlemmer, H.] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany.
[Belov, K.; Wissel, S. A.; Hoover, S.; Lam, J.; Saltzberg, D.; Urdaneta, D.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Belov, K.; Romero-Wolf, A.; Naudet, C. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Garcia-Fernandez, D.; Alvarez-Muniz, J.; Carvalho, W. R., Jr.; Zas, E.] Univ Santiago de Compostela, Dept Fis Particulas, Santiago De Compostela 15782, Spain.
[Garcia-Fernandez, D.; Alvarez-Muniz, J.; Carvalho, W. R., Jr.; Zas, E.] Univ Santiago de Compostela, Inst Galego Fis Altas Enerxias, Santiago De Compostela 15782, Spain.
[Bugaev, V.; Binns, W. R.; Dowkontt, P. F.; Israel, M. H.; Link, J. T.; Rauch, B. F.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Bugaev, V.; Binns, W. R.; Dowkontt, P. F.; Israel, M. H.; Link, J. T.; Rauch, B. F.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
[Wissel, S. A.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA.
[Allison, P.; Beatty, J. J.; Connolly, A.; Mercurio, B. C.; Palladino, K.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Barwick, S. W.; Goldstein, D.; Wu, F.] Univ Calif Irvine, Dept Phys, Irvine, CA 92697 USA.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Besson, D. Z.] Natl Res Nucl Univ, Moscow Engn Phys Inst, Moscow 115409, Russia.
[Chen, C.; Chen, P.] Natl Taiwan Univ, Grad Inst Astrophys, Dept Phys, Taipei 10617, Taiwan.
[Chen, C.; Chen, P.] Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys, Taipei 10617, Taiwan.
[Clem, J. M.; Javaid, A.; Mulrey, K.; Seckel, D.] Univ Delaware, Dept Phys, Newark, DE 19716 USA.
[Huegen, T.] Karlsruhe Inst Technol, Inst Kernphys, D-76344 Karlsruhe, Germany.
[Nichol, R. J.] UCL, Dept Phys & Astron, London WC1 EBT, England.
[Chen, P.; Field, R. C.; Hast, C.; Ng, J.; Reil, K.; Walz, D.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Walz, D.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Vieregg, A. G.] Univ Chicago, Kavli Inst Cosmol Phys, Dept Phys, Enrico Fermi Inst, Chicago, IL 60637 USA.
RP Schoorlemmer, H (reprint author), Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany.
EM harmscho@mpi-hd.mpg.de
RI zas, enrique/I-5556-2015; Alvarez-Muniz, Jaime/H-1857-2015; Beatty,
James/D-9310-2011;
OI zas, enrique/0000-0002-4430-8117; Alvarez-Muniz,
Jaime/0000-0002-2367-0803; Beatty, James/0000-0003-0481-4952; Lusczek,
Elizabeth/0000-0003-4680-965X
FU NASA; U.S. National Science Foundation; U.S. Department of Energy;
Columbia Scientific Balloon Facility; Ministerio de Economia
[FPA2012-39489]; Consolider-Ingenio CPAN Programme [CSD2007-00042];
Xunta de Galicia [GRC2013-024]; Feder Fundsand Marie Curie-IRSES/EPLANET
(European Particle physics Latin American NETwork); 7th Framework
Program [PIRSES-2009-GA-246806]
FX We would like to thank Marianne Ludwig from Karlsruhe Institute of
Technology for helpful discussions and in the early days of this work.
We are grateful to NASA, the U.S. National Science Foundation, the U.S.
Department of Energy, and the Columbia Scientific Balloon Facility for
their generous support of these efforts. We would like to extend our
thanks to the 2006-2007 on-ice LDB and McMurdo crews for their support.
Part of the research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. J.A.-M., W.R.C., D.G.-F., and E.Z.
thank Ministerio de Economia (FPA2012-39489), Consolider-Ingenio 2010
CPAN Programme (CSD2007-00042), Xunta de Galicia (GRC2013-024), Feder
Fundsand Marie Curie-IRSES/EPLANET (European Particle physics Latin
American NETwork), and 7th Framework Program (PIRSES-2009-GA-246806).
NR 39
TC 5
Z9 5
U1 5
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
EI 1873-2852
J9 ASTROPART PHYS
JI Astropart Phys.
PD APR
PY 2016
VL 77
BP 32
EP 43
DI 10.1016/j.astropartphys.2016.01.001
PG 12
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DH3GH
UT WOS:000372675000003
ER
PT J
AU Goue, OY
Raghothamachar, B
Yang, Y
Guo, JQ
Dudley, M
Kisslinger, K
Trunek, AJ
Neudeck, PG
Spry, DJ
Woodworth, AA
AF Goue, Ouloide Y.
Raghothamachar, Balaji
Yang, Yu
Guo, Jianqiu
Dudley, Michael
Kisslinger, Kim
Trunek, Andrew J.
Neudeck, Philip G.
Spry, David J.
Woodworth, Andrew A.
TI Study of Defect Structures in 6H-SiC a/m-Plane Pseudofiber Crystals
Grown by Hot-Wall CVD Epitaxy
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article
DE Silicon carbide; large tapered crystal; lateral expansion; hot-wall
chemical vapor deposition; x-ray topography; stacking faults
ID 4H-SIC SINGLE-CRYSTALS; HEATED FLOATING-ZONE; RAMAN-SCATTERING;
STACKING-FAULTS; DIODES
AB Structural perfection of silicon carbide (SiC) single crystals is essential to achieve high-performance power devices. A new bulk growth process for SiC proposed by researchers at NASA Glenn Research Center, called large tapered crystal (LTC) growth, based on axial fiber growth followed by lateral expansion, could produce SiC boules with potentially as few as one threading screw dislocation per wafer. In this study, the lateral expansion aspect of LTC growth is addressed through analysis of lateral growth of 6H-SiC a/m-plane seed crystals by hot-wall chemical vapor deposition. Preliminary synchrotron white-beam x-ray topography (SWBXT) indicates that the as-grown boules match the polytype structure of the underlying seed and have a faceted hexagonal morphology with a strain-free surface marked by steps. SWBXT Laue diffraction patterns of transverse and axial slices of the boules reveal streaks suggesting the existence of stacking faults/polytypes, and this is confirmed by micro-Raman spectroscopy. Transmission x-ray topography of both transverse and axial slices reveals inhomogeneous strains at the seed-epilayer interface and linear features propagating from the seed along the growth direction. Micro-Raman mapping of an axial slice reveals that the seed contains high stacking disorder, while contrast extinction analysis (g center dot b and g center dot bxl) of the linear features reveals that these are mostly edge-type basal plane dislocations. Further high-resolution transmission electron microscopy investigation of the seed-homoepilayer interface also reveals nanobands of different SiC polytypes. A model for their formation mechanism is proposed. Finally, the implication of these results for improving the LTC growth process is addressed.
C1 [Goue, Ouloide Y.; Raghothamachar, Balaji; Yang, Yu; Guo, Jianqiu; Dudley, Michael] SUNY Stony Brook, Dept Mat Sci & Engn, Stony Brook, NY 11794 USA.
[Kisslinger, Kim] Brookhaven Natl Lab, Ctr Funct Nanomat, Upton, NY 11793 USA.
[Trunek, Andrew J.; Neudeck, Philip G.; Spry, David J.; Woodworth, Andrew A.] NASA, Glenn Res Ctr, 21000 Brookpark Rd,MS 77-1, Cleveland, OH 44135 USA.
RP Goue, OY; Raghothamachar, B; Yang, Y; Guo, JQ; Dudley, M (reprint author), SUNY Stony Brook, Dept Mat Sci & Engn, Stony Brook, NY 11794 USA.; Kisslinger, K (reprint author), Brookhaven Natl Lab, Ctr Funct Nanomat, Upton, NY 11793 USA.; Trunek, AJ; Neudeck, PG; Spry, DJ; Woodworth, AA (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd,MS 77-1, Cleveland, OH 44135 USA.
EM ouloide.goue@stonybrook.edu; balaji.raghothamachar@stonybrook.edu;
yu.yang@stonybrook.edu; jqguo123@gmail.com;
michael.dudley@stonybrook.edu; kisslinger@bnl.gov;
Andrew.J.Trunek@nasa.gov; Neudeck@nasa.gov; David.J.Spry@nasa.gov;
Andrew.A.Woodworth@nasa.gov
FU NASA Glenn Research Center; US Department of Energy (DOE) [SAA3-1048,
DE-EE0001093/001]; NASA Postdoctoral Program Fellowship - NASA Vehicle
Systems Safety Technologies Project in the Aviation Safety Program; US
DOE [DE-AC02-76CH00016]; US DOE, Office of Basic Energy Sciences
[DE-AC02-98CH10886]
FX Work supported by NASA Glenn Research Center and the US Department of
Energy (DOE) Vehicle Technology Program via Space Act Agreement
(SAA3-1048) (DOE IA # DE-EE0001093/001) monitored by Susan Rogers (DOE),
and NASA Postdoctoral Program Fellowship supported by NASA Vehicle
Systems Safety Technologies Project in the Aviation Safety Program.
SWBXT work was carried out at Stony Brook Topography Facility (Beamline
X19C) at the NSLS, Brookhaven National Laboratory, which is supported by
the US DOE under Grant No. DE-AC02-76CH00016. HRTEM work carried out at
the Center for Functional Nanomaterials, Brookhaven National Laboratory,
which is supported by the US DOE, Office of Basic Energy Sciences, under
Contract No. DE-AC02-98CH10886. Raman scattering performed by Nicholas
Heller.
NR 25
TC 0
Z9 0
U1 5
U2 12
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
EI 1543-186X
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD APR
PY 2016
VL 45
IS 4
BP 2078
EP 2086
DI 10.1007/s11664-015-4185-7
PG 9
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA DH1KW
UT WOS:000372543900013
ER
PT J
AU Wallace, TT
Jin, ZH
Su, J
AF Wallace, T. T.
Jin, Z. -H.
Su, J.
TI Efficiency of a Sandwiched Thermoelectric Material with a Graded
Interlayer and Temperature-Dependent Properties
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article
DE Thermoelectric material; functionally graded material; segmented
material; energy conversion efficiency; temperature-dependent properties
AB This paper investigates the energy conversion efficiency for a sandwiched thermoelectric (TE) material with a graded interlayer and temperature-dependent properties. The graded interlayer can be modeled as a composite of the two homogeneous end material members to achieve continuously varying composition and properties, thus eliminating the electrical contact resistance at the interfaces of segmented TE materials. The temperature distribution and efficiency are obtained by a semianalytical recurrence relation and a simple iteration technique. In the numerical examples, we consider a sandwiched TE element consisting of nanostructured Bi2Te3 at the cold-end side, nanostructured PbTe at the hot-end side, and a graded interlayer of Bi2Te3-PbTe composite. The numerical results show that the peak efficiency of the sandwiched TE material with no contact resistance is higher than that of segmented Bi2Te3/PbTe with contact resistance at the sharp interface between Bi2Te3 and PbTe. The peak efficiency of the sandwiched material is also influenced by the location of and gradation profile in the graded interlayer. Finally, it is found that temperature dependence of properties decreases the efficiencies of Bi2Te3 and PbTe.
C1 [Wallace, T. T.; Jin, Z. -H.] Univ Maine, Dept Mech Engn, Orono, ME 04469 USA.
[Wallace, T. T.] Maine Maritime Acad, Marine Engine Testing & Emiss Lab, Castine, ME 04420 USA.
[Su, J.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
RP Jin, ZH (reprint author), Univ Maine, Dept Mech Engn, Orono, ME 04469 USA.
EM zhihe.jin@maine.edu
FU NASA EPSCoR through the Maine Space Grant Consortium; US DOT UTC under
the METEL lab of Maine Maritime Academy [DTRT13-G-UTC43]
FX The work described in this paper is supported by NASA EPSCoR through the
Maine Space Grant Consortium and the US DOT UTC Grant DTRT13-G-UTC43
under the METEL lab of Maine Maritime Academy.
NR 17
TC 0
Z9 0
U1 4
U2 17
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
EI 1543-186X
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD APR
PY 2016
VL 45
IS 4
BP 2142
EP 2149
DI 10.1007/s11664-016-4358-z
PG 8
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA DH1KW
UT WOS:000372543900022
ER
PT J
AU Dirmeyer, PA
Wu, JX
Norton, HE
Dorigo, WA
Quiring, SM
Ford, TW
Santanello, JA
Bosilovich, MG
Ek, MB
Koster, RD
Balsamo, G
Lawrence, DM
AF Dirmeyer, Paul A.
Wu, Jiexia
Norton, Holly E.
Dorigo, Wouter A.
Quiring, Steven M.
Ford, Trenton W.
Santanello, Joseph A., Jr.
Bosilovich, Michael G.
Ek, Michael B.
Koster, Randal D.
Balsamo, Gianpaolo
Lawrence, David M.
TI Confronting Weather and Climate Models with Observational Data from Soil
Moisture Networks over the United States
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Reanalysis data; Land surface model; Geographic location/entity; Soil
moisture; Climate models; Instrumentation/sensors; Physical Meteorology
and Climatology; North America; Models and modeling; Observational
techniques and algorithms
ID DATA ASSIMILATION SYSTEM; LAND-SURFACE MODELS; REANALYSIS DATA SET;
SPATIAL VARIABILITY; TRIPLE COLLOCATION; COUPLING STRENGTH; OBSERVING
SYSTEM; PERFORMANCE; VALIDATION; MESONET
AB Four land surface models in uncoupled and coupled configurations are compared to observations of daily soil moisture from 19 networks in the conterminous United States to determine the viability of such comparisons and explore the characteristics of model and observational data. First, observations are analyzed for error characteristics and representation of spatial and temporal variability. Some networks have multiple stations within an area comparable to model grid boxes; for those it is found that aggregation of stations before calculation of statistics has little effect on estimates of variance, but soil moisture memory is sensitive to aggregation. Statistics for some networks stand out as unlike those of their neighbors, likely because of differences in instrumentation, calibration, and maintenance. Buried sensors appear to have less random error than near-field remote sensing techniques, and heat-dissipation sensors show less temporal variability than other types. Model soil moistures are evaluated using three metrics: standard deviation in time, temporal correlation (memory), and spatial correlation (length scale). Models do relatively well in capturing large-scale variability of metrics across climate regimes, but they poorly reproduce observed patterns at scales of hundreds of kilometers and smaller. Uncoupled land models do no better than coupled model configurations, nor do reanalyses outperform free-running models. Spatial decorrelation scales are found to be difficult to diagnose. Using data for model validation, calibration, or data assimilation from multiple soil moisture networks with different types of sensors and measurement techniques requires great caution. Data from models and observations should be put on the same spatial and temporal scales before comparison.
C1 [Dirmeyer, Paul A.; Wu, Jiexia; Norton, Holly E.] George Mason Univ, Fairfax, VA 22030 USA.
[Dorigo, Wouter A.] Vienna Univ Technol, A-1040 Vienna, Austria.
[Dorigo, Wouter A.] Univ Ghent, Lab Forest & Water Management, B-9000 Ghent, Belgium.
[Quiring, Steven M.] Texas A&M Univ, College Stn, TX USA.
[Ford, Trenton W.] So Illinois Univ, Carbondale, IL 62901 USA.
[Santanello, Joseph A., Jr.; Bosilovich, Michael G.; Koster, Randal D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Ek, Michael B.] NOAA, Natl Ctr Environm Predict, College Pk, MD USA.
[Balsamo, Gianpaolo] European Ctr Medium Range Weather Forecasts, Shinfield Pk, Reading RG2 9AX, Berks, England.
[Lawrence, David M.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
RP Dirmeyer, PA (reprint author), George Mason Univ, Ctr Ocean Land Atmosphere Studies, 4400 Univ Dr,Mail Stop 6C5, Fairfax, VA 22030 USA.
EM pdirmeye@gmu.edu
RI Koster, Randal/F-5881-2012; Santanello, Joseph/D-4438-2012; Bosilovich,
Michael/F-8175-2012
OI Koster, Randal/0000-0001-6418-6383; Santanello,
Joseph/0000-0002-0807-6590;
FU National Aeronautics and Space Administration [NNX13AQ21G]; SMOS Soil
Moisture Network Study Operational Phase (ESA ESTEC) [4000102722/10]
FX This work has been primarily supported by National Aeronautics and Space
Administration Grant NNX13AQ21G. Funding for W.D. has come from SMOS
Soil Moisture Network Study Operational Phase (ESA ESTEC Contract
4000102722/10). Support for the Twentieth Century Reanalysis Project
dataset is provided by the U.S. Department of Energy, Office of Science
Innovative and Novel Computational Impact on Theory and Experiment (DOE
INCITE) program, and Office of Biological and Environmental Research
(BER), and by the National Oceanic and Atmospheric Administration
Climate Program Office. We thank G. Compo for making 20CR data available
to us.
NR 66
TC 4
Z9 4
U1 2
U2 10
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD APR
PY 2016
VL 17
IS 4
BP 1049
EP 1067
DI 10.1175/JHM-D-15-0196.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DG9LY
UT WOS:000372405700001
ER
PT J
AU Tejero, EF
Doerffer, P
Szule, O
Crosse, JL
AF Tejero, F. E.
Doerffer, P.
Szule, O.
Crosse, J. L.
TI Numerical Simulation of the Tip Aerodynamics and Acoustics Test
SO JOURNAL OF THERMAL SCIENCE
LA English
DT Article
DE AH-1G; TAAT; helicopter rotor; forward flight; chimera overlapping grid
ID HELICOPTER ROTOR BLADE; FREE-WAKE
AB The application of an efficient flow control system on helicopter rotor blades may lead to improved aerodynamic performance. Recently, our invention of Rod Vortex Generators (RVGs) has been analyzed for helicopter rotor blades in hover with success. As a step forward, the study has been extended to forward flight conditions. For this reason, a validation of the numerical modelling for a reference helicopter rotor (without flow control) is needed. The article presents a study of the flow-field of the AH-1G helicopter rotor in low-, medium- and high-speed forward flight. The CFD code FLOWer from DLR has proven to be a suitable tool for the aerodynamic analysis of the two-bladed rotor without any artificial wake modelling. It solves the URANS equations with LEA (Linear Explicit Algebraic stress) k-omega model using the chimera overlapping grids technique. Validation of the numerical model uses comparison with the detailed flight test data gathered by Cross J. L. and Watts M. E. during the Tip Aerodynamics and Acoustics Test (TAAT) conducted at NASA in 1981. Satisfactory agreements for all speed regimes and a presence of significant flow separation in high-speed forward flight suggest a possible benefit from the future implementation of RVGs. The numerical results based on the URANS approach are presented not only for a popular, low-speed case commonly used in rotorcraft community for CFD codes validation but preferably for medium- and high-speed test conditions that have not been published to date.
C1 [Tejero, F. E.; Doerffer, P.; Szule, O.] Polish Acad Sci, Szwalski Inst Fluid Flow Machinery, Fiszera 14, PL-80231 Gdansk, Poland.
[Crosse, J. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Doerffer, P (reprint author), Polish Acad Sci, Szwalski Inst Fluid Flow Machinery, Fiszera 14, PL-80231 Gdansk, Poland.
FU 7th Framework Programme project IMESCON [PITN-GA-2010-264672]; PL-Grid
Infrastructure
FX This work was supported by the 7th Framework Programme project IMESCON
(PITN-GA-2010-264672) and in part by PL-Grid Infrastructure.
NR 18
TC 0
Z9 0
U1 1
U2 8
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1003-2169
EI 1993-033X
J9 J THERM SCI
JI J. Therm. Sci.
PD APR
PY 2016
VL 25
IS 2
BP 153
EP 160
DI 10.1007/s11630-016-0846-y
PG 8
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA DG9DI
UT WOS:000372382600007
ER
PT J
AU Ju, JC
Masek, JG
AF Ju, Junchang
Masek, Jeffrey G.
TI The vegetation greenness trend in Canada and US Alaska from 1984-2012
Landsat data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Landsat; NDVI; Vegetation greenness trend; Tundra; Boreal forest; AVHRR
ID SATELLITE DATA; SURFACE REFLECTANCE; SHRUB EXPANSION; NORTH-AMERICA;
COVER CHANGE; TIME-SERIES; NDVI TRENDS; FOREST; DISTURBANCE; LATITUDES
AB To assess the North American high-latitude vegetation response to the rising temperature, we derived NDVI trend for 91.2% of the non-water, non-snow land area of Canada and Alaska using the peak-summer Landsat surface reflectance data of 1984-2012. Our analysis indicated that 29.4% and 2.9% of the land area of Canada and Alaska showed statistically significant positive (greening) and negative (browning) trends respectively, at significance level p < 0.01, after burned forest areas were masked out. The area with greening trend dominated over that with browning trend for all land cover types. The greening occurred primarily in the tundra of western Alaska, along the north coast of Canada and in northeastern Canada; the most intensive and extensive greening occurred in Quebec and Labrador. The browning occurred mostly in the boreal forests of eastern Alaska. The Landsat-based greenness trend is broadly similar to the 8-km GIMMS AVHRR-based trend for all vegetation zones. However, for tundra, the Landsat data indicated much less extensive greening in Alaska North Slope and much more extensive greening in Quebec and Labrador, and substantially less extensive browning trend in the boreal forests that were free of fire disturbances. These differences call for further validation of the Landsat reflectance and the AVHRR NDVI datasets. Correlation study with local environmental factors, such as topography, glacial history and soil condition, will be needed to understand the heterogeneous greenness change at the Landsat scale. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Ju, Junchang] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Ju, Junchang; Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab Code 618, Greenbelt, MD 20771 USA.
RP Ju, JC (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA.
EM junchang.ju@nasa.gov
RI Masek, Jeffrey/D-7673-2012
FU NASA Terrestrial Ecology program
FX We thank Mark Carroll for sharing the Landsat data, the collection of
which had required a sustained effort. We thank Mark Friedl and Damien
Sulla-Menashe for their constructive discussion on the results and the
three reviewers for their comments and suggestions that greatly improved
the quality of the paper. This research was supported by the NASA
Terrestrial Ecology program, and the computation was conducted in the
high performance computing environment Advanced Data Analytics Platform
(ADAPT) at the NASA Center for Climate Simulation.
NR 45
TC 15
Z9 15
U1 18
U2 62
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD APR
PY 2016
VL 176
BP 1
EP 16
DI 10.1016/j.rse.2016.01.001
PG 16
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DG9DO
UT WOS:000372383200001
ER
PT J
AU Roy, DP
Zhang, HK
Ju, J
Gomez-Dans, JL
Lewis, PE
Schaaf, CB
Sun, Q
Li, J
Huang, H
Kovalskyy, V
AF Roy, D. P.
Zhang, H. K.
Ju, J.
Gomez-Dans, J. L.
Lewis, P. E.
Schaaf, C. B.
Sun, Q.
Li, J.
Huang, H.
Kovalskyy, V.
TI A general method to normalize Landsat reflectance data to nadir BRDF
adjusted reflectance
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Bidirectional reflectance distribution function (BRDF); Landsat; NBAR;
MODIS
ID CONTERMINOUS UNITED-STATES; ORBIT GEOMETRIC CALIBRATION; PLUS
ATMOSPHERIC CORRECTION; FOREST-COVER CHANGE; BIDIRECTIONAL REFLECTANCE;
SURFACE REFLECTANCE; TM IMAGERY; DATA SETS; MODIS; MODEL
AB The Landsat satellites have been providing spectacular imagery of the Earth's surface for over 40 years. However, they acquire images at view angles 7.5 degrees from nadir that cause small directional effects in the surface reflectance. There are also variations with solar zenith angle over the year that can cause apparent change in reflectance even if the surface properties remain constant. When Landsat data from adjoining paths, or from long time series are used, a model of the surface anisotropy is required to adjust all Landsat observations to a uniform nadir view (primarily for visual consistency, vegetation monitoring, or detection of subtle surface changes). Here a generalized approach is developed to provide consistent view angle corrections across the Landsat archive. While this approach is not applicable for generation of Landsat surface albedo, which requires a full characterization of the surface bidirectional reflectance distribution function (BRDF), or for correction to a constant solar illumination angle across a wide range of sun angles, it provides Landsat nadir BRDF-adjusted reflectance (NBAR) for a range of terrestrial monitoring applications.
The Landsat NBAR is derived as the product of the observed Landsat reflectance and the ratio of the reflectances modeled using MODIS BRDF spectral model parameters for the observed Landsat and for a nadir view and fixed solar zenith geometry. In this study, a total of 567 conterminous United States (CONUS) January and July 2010 Landsat 5 Thematic Mapper (TM) and Landsat 7 Enhanced Thematic Mapper (ETM+) images that have swath edge overlapping paths sensed in alternating backscatter and forward scattering orientations were used. The average difference between Landsat 5 TM and Landsat 7 ETM + surface reflectance in the forward and backward scatter directions at the overlapping Landsat scan edges was quantified. The CONUS July view zenith BRDF effects were about 0.02 in the Landsat visible bands, and about 0.03, 0.05 and 0.06, in the 2.1 mu m, 1.6 mu m and near infrared bands respectively. Comparisons of Landsat 5 TM and Landsat 7 ETM + NBAR derived using MODIS BRDF spectral model parameters defined with respect to different spatial and temporal scales, and defined with respect to different land cover types, were undertaken. The results suggest that, because the BRDF shapes of different terrestrial surfaces are sufficiently similar over the narrow 15 Landsat field of view, a fixed set of MODIS BRDF spectral model parameters may be adequate for Landsat NBAR derivation with little sensitivity to the land cover type, condition, or surface disturbance. A fixed set of BRDF spectral model parameters, derived from a global year of highest quality snow-free MODIS BRDF product values, are provided so users may implement the described Landsat NBAR generation method. (C) 2016 The Authors. Published by Elsevier Inc.
C1 [Roy, D. P.; Zhang, H. K.; Li, J.; Huang, H.; Kovalskyy, V.] S Dakota State Univ, Geospatial Sci Ctr Excellence, Brookings, SD 57007 USA.
[Ju, J.] Univ Space Res Assoc, 7178 Columbia Gateway Dr, Columbia, MD 21046 USA.
[Ju, J.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Gomez-Dans, J. L.; Lewis, P. E.] NERC Natl Ctr Earth Observat NCEO, London, England.
[Gomez-Dans, J. L.; Lewis, P. E.] UCL, Dept Geog, Gower St, London WC1E 6BT, England.
[Schaaf, C. B.; Sun, Q.] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA.
RP Roy, DP (reprint author), S Dakota State Univ, Geospatial Sci Ctr Excellence, Brookings, SD 57007 USA.
RI Sun, Qingsong/I-9040-2016
OI Sun, Qingsong/0000-0002-7710-2123
FU U.S. Department of Interior, U.S. Geological Survey (USGS) [G12PC00069];
NASA Making Earth System Data Records for Use in Research Environments
(MEaSUREs) program [NNX13AJ24A]; NASA MODIS BRDF/Albedo/NBAR product
generation grant [NNX12AL38G]
FX This research was funded by the U.S. Department of Interior, U.S.
Geological Survey (USGS) under grant G12PC00069, by the NASA Making
Earth System Data Records for Use in Research Environments (MEaSUREs)
program under Cooperative Agreement NNX13AJ24A, and by the NASA MODIS
BRDF/Albedo/NBAR product generation grant NNX12AL38G. The U.S. Landsat
project management and staff at USGS Earth Resources Observation and
Science (EROS) Center, Sioux Falls, South Dakota, are thanked for
provision of the Landsat data.
NR 82
TC 10
Z9 10
U1 7
U2 23
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD APR
PY 2016
VL 176
BP 255
EP 271
DI 10.1016/j.rse.2016.01.023
PG 17
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DG9DO
UT WOS:000372383200020
ER
PT J
AU Sumnall, M
Peduzzi, A
Fox, TR
Wynne, RH
Thomas, VA
Cook, B
AF Sumnall, Matthew
Peduzzi, Alicia
Fox, Thomas R.
Wynne, Randolph H.
Thomas, Valerie A.
Cook, Bruce
TI Assessing the transferability of statistical predictive models for leaf
area index between two airborne discrete return LiDAR sensor designs
within multiple intensely managed Loblolly pine forest locations in the
south-eastern USA
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Loblolly pine; Forest management; LiDAR; Remote sensing; Leaf area index
ID LASER-SCANNING DATA; WAVE-FORM LIDAR; VEGETATION INDEXES; LAI;
EVAPOTRANSPIRATION; INVENTORY; DENSITY; METRICS; LEAVES
AB Leaf area is an important forest structural variable which serves as the primary means of mass and energy exchange within vegetated ecosystems. The objective of the current study was to determine if leaf area index (LAI) could be estimated accurately and consistently in five intensively managed pine plantation forests using two multiple-return airborne LiDAR datasets. Field measurements of LAI were made using the LiCOR LAI2000 and LAI2200 instruments within 116 plots were established of varying size and within a variety of stand conditions (i.e. stand age, nutrient regime and stem density) in North Carolina and Virginia in 2008 and 2013. A number of common LiDAR return height and intensity distribution metrics were calculated (e.g. average return height), in addition to ten indices, with two additional variants, utilized in the surrounding literature which have been used to estimate LAI and fractional cover, were calculated from return heights and intensity, for each plot extent. Each of the indices was assessed for correlation with each other, and was used as independent variables in linear regression analysis with field LAI as the dependent variable. All LiDAR derived metrics were also entered into a forward stepwise linear regression. The results from each of the indices varied from an R-2 of 0.33 (S.E. 0.87) to 0.89 (S.E. 0.36). Those indices calculated using ratios of all returns produced the strongest correlations, such as the Above and Below Ratio Index (ABRI) and Laser Penetration Index 1 ( LPI1). The regression model produced from a combination of three metrics did not improve correlations greatly (R-2 0.90; S.E. 0.35). The results indicate that LAI can be predicted over a range of intensively managed pine plantation forest environments accurately when using different LiDAR sensor designs. Those indices which incorporated counts of specific return numbers (e.g. first returns) or return intensity correlated poorly with field measurements. There were disparities between the number of different types of returns and intensity values when comparing the results from two LiDAR sensors, indicating that predictive models developed using such metrics are not transferable between datasets with different acquisition parameters. Each of the indices were significantly correlated with one another, with one exception (LAI proxy), in particular those indices calculated from all returns, which indicates similarities in information content for those indices. It can then be argued that LiDAR indices have reached a similar stage in development to those calculated from optical-spectral sensors, but which offer a number of advantages, such as the reduction or removal of saturation issues in areas of high biomass. Published by Elsevier Inc.
C1 [Sumnall, Matthew; Fox, Thomas R.] Virginia Polytech Inst & State Univ, Dept Forest Resources & Environm Conservat, 228 Cheatham Hall,Mail Code 0324, Blacksburg, VA 24061 USA.
[Peduzzi, Alicia] US Forest Serv, USDA, 507,25th St, Ogden, UT 84401 USA.
[Wynne, Randolph H.] Virginia Polytech Inst & State Univ, Dept Forest Resources & Environm Conservat, 319 Cheatham Hall,Mail Code 0324, Blacksburg, VA 24061 USA.
[Thomas, Valerie A.] Virginia Polytech Inst & State Univ, Dept Forest Resources & Environm Conservat, 307A Cheatham Hall,Mail Code 0324, Blacksburg, VA 24061 USA.
[Cook, Bruce] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
RP Sumnall, M (reprint author), Virginia Polytech Inst & State Univ, Dept Forest Resources & Environm Conservat, 228 Cheatham Hall,Mail Code 0324, Blacksburg, VA 24061 USA.
FU Virginia Agricultural Experiment Station [VA-136623]; Program McIntire
Stennis of the National Institute of Food and Agriculture, U.S.
Department of Agriculture; Forest Productivity Cooperative; NASA
FX This research was possible thanks to the support from the Forest
Productivity Cooperative, the help in field data collection provided by
Beth Stein and the assistance Alica Peduzzi, who provided the field data
for validation of the 2008 LiDAR acquisition assessed in the project. We
gratefully acknowledge the support and LiDAR data supplied by NASA, in
addition to the support of the staff members of the Duke Forest teaching
and research laboratory, the Northern Research Station Strategic
Foresight Group of the North Carolina Forest service and the landowner
Weyerhaeuser. Funding for this work was provided in part by the Virginia
Agricultural Experiment Station (Project Number VA-136623) and the
Program McIntire Stennis of the National Institute of Food and
Agriculture, U.S. Department of Agriculture.
NR 49
TC 2
Z9 3
U1 5
U2 19
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD APR
PY 2016
VL 176
BP 308
EP 319
DI 10.1016/j.rse.2016.02.012
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DG9DO
UT WOS:000372383200024
ER
PT J
AU D'Souza, SN
Sarigul-Khjn, N
AF D'Souza, Sarah N.
Sarigul-Khjn, Nesrin
TI A trajectory generation framework for modeling spacecraft entry in MDAO
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Spacecraft entry; Guidance; MDAO; Optimization
ID GUIDANCE; VEHICLES; AEROCAPTURE
AB In this paper a novel trajectory generation framework was developed that optimizes trajectory event conditions for use in a Generalized Entry Guidance algorithm. The framework was developed to be adaptable via the use of high fidelity equations of motion and drag based analytical bank profiles. Within this framework, a novel technique was implemented that resolved the sensitivity of the bank profile to atmospheric nonlinearities. The framework's adaptability was established by running two different entry bank conditions. Each case yielded a reference trajectory and set of transition event conditions that are flight feasible and implementable in a Generalized Entry Guidance algorithm. (C) 2016 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [D'Souza, Sarah N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Sarigul-Khjn, Nesrin] Univ Calif Davis, Mech & Aerosp Engn Dept, Space Engn Res & Grad Program SpaceED, Davis, CA 95616 USA.
RP Sarigul-Khjn, N (reprint author), Univ Calif Davis, Mech & Aerosp Engn Dept, Space Engn Res & Grad Program SpaceED, Davis, CA 95616 USA.
EM sarah.n.dsouza@nasa.gov; nsarigulklijn@ucdavis.edu
NR 52
TC 0
Z9 0
U1 3
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD APR-MAY
PY 2016
VL 121
BP 95
EP 109
DI 10.1016/j.actaastro.2015.12.017
PG 15
WC Engineering, Aerospace
SC Engineering
GA DG1OV
UT WOS:000371838300011
ER
PT J
AU Sayenko, DG
Miller, TF
Melnik, KA
Netreba, AI
Khusnutdinova, DR
Kitov, VV
Tomilovskaya, ES
Reschke, MF
Gerasimenko, YP
Kozlovskaya, IB
AF Sayenko, D. G.
Miller, T. F.
Melnik, K. A.
Netreba, A. I.
Khusnutdinova, D. R.
Kitov, V. V.
Tomilovskaya, E. S.
Reschke, M. F.
Gerasimenko, Y. P.
Kozlovskaya, I. B.
TI Acute effects of Dry Immersion on kinematic characteristics of postural
corrective responses
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Human; Balance; Postural corrective responses; Microgravity; Dry
Immersion; Weight-bearing
ID VISUO-MOTOR SKILL; SOLEUS H-REFLEX; SPACE-FLIGHT; MICROGRAVITY; HUMANS;
MUSCLE; ADAPTATIONS; ACTIVATION; STIMULATION; SENSITIVITY
AB Impairments in balance control are inevitable following exposure to microgravity. However, the role of particular sensory system in postural disorders at different stages of the exposure to microgravity still remains unknown. We used a method called Dry Immersion (DI), as a ground-based model of microgravity, to elucidate the effects of 6-h of load related afferent inputs on kinematic characteristics of postural corrective responses evoked by pushes to the chest of different intensities during upright standing. The structure of postural corrective responses was altered following exposure to DI, which was manifested by: (1) an increase of the ankle and knee flexion during perturbations of medium intensity, (2) the lack of the compensatory hip extension, as well as diminished knee and ankle flexion with a further increase of the perturbation intensity to submaximal level. We suggest that the lack of weight-bearing increases the reactivity of the balance control system, whereas the ability to scale the responses proportionally to the perturbation intensity decreases. Disrupted neuromuscular coordination of postural corrective responses following DI can be attributed to adaptive neural modifications on the spinal and cortical levels. The present study provides evidence that even a short-term lack of load-related afferent inputs alters kinematic patterns of postural corrective responses, and can result in decreased balance control. Because vestibular input is not primarily affected during the DI exposure, our results indicate that activity and the state of the load-related afferents play critical roles in balance control following real or simulated microgravity. (C) 2016 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Sayenko, D. G.; Miller, T. F.; Melnik, K. A.; Netreba, A. I.; Khusnutdinova, D. R.; Kitov, V. V.; Tomilovskaya, E. S.; Kozlovskaya, I. B.] Russian Acad Sci, Inst Biomed Problems, Russian Federat State Sci Ctr, Moscow, Russia.
[Sayenko, D. G.; Gerasimenko, Y. P.] Univ Calif Los Angeles, Dept Integrat Biol & Physiol, 610 Charles E Young Dr East, Los Angeles, CA 90095 USA.
[Reschke, M. F.] NASA, Lyndon B Johnson Space Ctr, Neurosci Lab, Houston, TX 77058 USA.
[Gerasimenko, Y. P.] Pavlov Inst Physiol, St Petersburg, Russia.
RP Sayenko, DG (reprint author), Univ Calif Los Angeles, Dept Integrat Biol & Physiol, 610 Charles E Young Dr East, Los Angeles, CA 90095 USA.
EM dsayenko@ucla.edu
RI Kozlovskaya, Inesa/R-9729-2016
FU Russian Science Foundation [15-15-20036]; Russian Foundation for Basic
Research Grant [13-04-12091-ofi-m-2013]
FX We would like to thank the research volunteers for their valuable
contributions to this study. We are grateful to Dr. Erica Dale for
reviewing the syntax. The analysis of the results performed by SDG was
supported by Russian Science Foundation (grant No. 15-15-20036). Partial
support for the data analysis and interpretation was provided to EST and
IBK by Russian Foundation for Basic Research Grant No.
13-04-12091-ofi-m-2013.
NR 47
TC 0
Z9 0
U1 3
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD APR-MAY
PY 2016
VL 121
BP 110
EP 115
DI 10.1016/j.actaastro.2015.12.054
PG 6
WC Engineering, Aerospace
SC Engineering
GA DG1OV
UT WOS:000371838300012
ER
PT J
AU Rape, A
Kulkarni, A
Bhat, B
Singh, J
AF Rape, A.
Kulkarni, A.
Bhat, B.
Singh, J.
TI Thermal reliability of copper alloy-diamond composites produced by
field-assisted sintering technology
SO JOURNAL OF COMPOSITE MATERIALS
LA English
DT Article
DE Copper-diamond; field assisted sintering technology; cycling; thermal
reliability; thermal conductivity
ID CU/DIAMOND COMPOSITES; MANAGEMENT MATERIALS; CONDUCTIVITY; PARTICLES
AB This paper highlights the thermal properties of copper-diamond composites fabricated by field assisted sintering technology. The samples were fabricated using a matrix of copper alloyed with silver and zirconium. Previous reports have shown that these samples possess high thermal conductivity. This work examines the thermal conductivity of the samples after being subjected to thermal cycling. Coefficient of thermal expansion is also reported in this work.
C1 [Rape, A.; Singh, J.] Penn State Univ, Appl Res Lab, 11650 Mapleridge Dr, North Royalton, OH 44133 USA.
[Kulkarni, A.] Penn State Univ, Dept Mech Engn, University Pk, PA 16802 USA.
[Bhat, B.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Rape, A (reprint author), Penn State Univ, Appl Res Lab, 11650 Mapleridge Dr, North Royalton, OH 44133 USA.
EM amr340@psu.edu
NR 12
TC 0
Z9 0
U1 3
U2 10
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0021-9983
EI 1530-793X
J9 J COMPOS MATER
JI J. Compos Mater.
PD APR
PY 2016
VL 50
IS 9
BP 1241
EP 1245
DI 10.1177/0021998315590263
PG 5
WC Materials Science, Composites
SC Materials Science
GA DG7ZF
UT WOS:000372301500009
ER
PT J
AU Morag, N
Williford, KH
Kitajima, K
Philippot, P
Van Kranendonk, MJ
Lepot, K
Thomazo, C
Valley, JW
AF Morag, Navot
Williford, Kenneth H.
Kitajima, Kouki
Philippot, Pascal
Van Kranendonk, Martin J.
Lepot, Kevin
Thomazo, Christophe
Valley, John W.
TI Microstructure-specific carbon isotopic signatures of organic matter
from similar to 3.5 Ga cherts of the Pilbara Craton support a biologic
origin
SO PRECAMBRIAN RESEARCH
LA English
DT Article
DE Dresser Formation; Organic matter; Carbon isotope ratio; SIMS;
Microfossils; Pilbara craton
ID NORTH-POLE AREA; INDIVIDUAL PRECAMBRIAN MICROFOSSILS; MICROBIAL SULFATE
REDUCTION; ISUA SUPRACRUSTAL BELT; EARTHS OLDEST FOSSILS; EARLY ARCHEAN
ERA; WESTERN-AUSTRALIA; DRESSER FORMATION; APEX CHERT; EARLY-LIFE
AB The similar to 3.5 Ga Dresser Formation from the North Pole Dome of the Pilbara Craton (Western Australia) contains some of the oldest evidence for life on Earth. Here, we present a detailed study of microstructure specific carbon isotopic composition of organic matter (OM) preserved in Dresser Formation bedded cherts and hydrothermal chert vein using in situ Secondary-Ion Mass Spectrometry (SIMS). The OM in these rocks occurs mainly as clots that, together with minor fine OM layers and laminae, are considered primary textures formed prior to host rock lithification. Other than rare OM-rich stylolites, no evidence was found for later OM migration beyond the micrometer scale. Average delta C-13(OM) values in specific microstructural types range between -33.6%. and -25.7%.. No correlation is seen between measured delta C-13 values and H/C ratios in the studied OM microstructures. This lack of correlation and the low metamorphic grade of the rocks studied argue against significant modification of OM isotopic composition by later metamorphic alteration. It is thus concluded that the range of delta C-13 values found in the samples represents primary OM isotopic variability. Within some individual samples variable delta C-13(OM) values are correlated with specific microstructural types. This observation is not consistent with solely abiotic OM formation via Fisher-Tropsch type reactions. When compared with associated delta C-13(ankerite) values, average delta C-13(OM) values indicate C isotopic fractionation [Delta C-13(Ank-OM)] of 25-33 parts per thousand, which translates to dissolved CO2-OM isotopic fractionation [Delta C-13(CO2-OM)] of 20-30 parts per thousand. This range of delta C-13(CO2-OM) is consistent with enzymatic C fixation via the Calvin cycle utilized by photoautotrophs and the reductive acetyl-CoA pathway utilized by chemolithoautotrophs. Photosynthetic OM formation is supported by the relatively shallow water depth inferred for the Dresser environment and the restricted occurrence of stromatolites to shallow water deposits in this unit, whereas chemolithosynthesis is supported by the abundance of OM in sub-seafloor hydrothermal chert veins. The range of delta C-13(OM) values observed in the samples may therefore represent the remains of different organisms utilizing different C-fixation pathways. Other biologic effects, such as the growth rate and density of microbial communities, and further heterotrophic overprinting of the autotrophic biomass may have also contributed to the observed range of delta C-13(OM) values. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Morag, Navot; Williford, Kenneth H.; Kitajima, Kouki; Lepot, Kevin; Valley, John W.] Univ Wisconsin, Dept Geosci, WiscSIMS, NASA Astrobiol Inst, 1215 W Dayton St, Madison, WI 53706 USA.
[Williford, Kenneth H.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Philippot, Pascal; Thomazo, Christophe] CNRS, Inst Phys Globe Paris, 4 Pl Jussieu, F-75005 Paris, France.
[Philippot, Pascal; Thomazo, Christophe] Univ Paris 07, 4 Pl Jussieu, F-75005 Paris, France.
[Van Kranendonk, Martin J.] Univ New South Wales Australia, Sch Biol Earth & Environm Sci, Kensington, NSW 2052, Australia.
[Van Kranendonk, Martin J.] Univ New South Wales Australia, Australian Ctr Astrobiol, Kensington, NSW 2052, Australia.
[Lepot, Kevin] Univ Lille 1, Lab Geosyst, CNRS UMR8217, F-59655 Villeneuve Dascq, France.
[Thomazo, Christophe] Univ Bourgogne, UMR CNRS Biogeosci UFR Sci Vie Terre Environm uB5, 6 Blvd Gabriel, F-21000 Dijon, France.
RP Morag, N (reprint author), Univ Wisconsin, Dept Geosci, WiscSIMS, NASA Astrobiol Inst, 1215 W Dayton St, Madison, WI 53706 USA.
EM morag@wisc.edu
RI Lepot, Kevin/C-7072-2014
OI Lepot, Kevin/0000-0003-0556-0405
FU NASA Astrobiology Institute; Labex UnivEarths program of Sorbonne Paris
Cite [ANR-10-LABX-0023, ANR-11-IDEX-0005-02]; National Aeronautics and
Space Administration; University of New South Wales; [NSF-EAR-1053466];
[NSF-EAR-1355590]
FX We thank Noriko Kita and Jim Kern for assistance with the ion
microprobe, John Fournelle,and Phil Gopon for assistance with the SEM
and EPMA, Maciej Sliwinski for assistance with the carbonate SIMS
standards and data processing, and Brian Hess for expert sample
preparation. Chris House provided our standard chip of PPRG-215. Funding
for this study was provided by the NASA Astrobiology Institute (NM, KW,
KK, KL, JV) and the Labex UnivEarths program of Sorbonne Paris Cite
(ANR-10-LABX-0023 and ANR-11-IDEX-0005-02, PP, KL, CT). Work by KW at
the Jet Propulsion Laboratory, California Institute of Technology was
funded by a grant from the National Aeronautics and Space
Administration. MVK acknowledges support from the University of New
South Wales. The WiscSIMS Lab is partly supported by NSF-EAR-1053466,
-1355590. Drillcore samples were made available through the
collaborative PDP drilling project organized by the Institute de
Physique de Globe de Paris and the Geological Survey of Western
Australia. This is contribution 699 from the Australian Research Council
Centre of Excellence for Core to Crust Fluid Systems.
NR 96
TC 0
Z9 0
U1 5
U2 18
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0301-9268
EI 1872-7433
J9 PRECAMBRIAN RES
JI Precambrian Res.
PD APR
PY 2016
VL 275
BP 429
EP 449
DI 10.1016/j.precamres.2016.01.014
PG 21
WC Geosciences, Multidisciplinary
SC Geology
GA DG1QC
UT WOS:000371841600026
ER
PT J
AU Buchheit, TE
Susan, DF
Massad, JE
Mcelhanon, JR
Noebe, RD
AF Buchheit, Thomas E.
Susan, Donald F.
Massad, Jordan E.
Mcelhanon, James R.
Noebe, Ronald D.
TI Mechanical and Functional Behavior of High-Temperature Ni-Ti-Pt Shape
Memory Alloys
SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND
MATERIALS SCIENCE
LA English
DT Article
AB A series of Ti-rich Ni-Ti-Pt ternary alloys with 13 to 18 at. pct Pt were processed by vacuum arc melting and characterized for their transformation behavior to identify shape memory alloys (SMA) that undergo transformation between 448 K and 498 K (175 A degrees C and 225 A degrees C) and achieve recoverable strain exceeding 2 pct. From this broader set of compositions, three alloys containing 15.5 to 16.5 at. pct Pt exhibited transformation temperatures in the vicinity of 473 K (200 A degrees C), thus were targeted for more detailed characterization. Preliminary microstructural evaluation of these three compositions revealed a martensitic microstructure with small amounts of Ti-2(Ni,Pt) particles. Room temperature mechanical testing gave a response characteristic of martensitic de-twinning followed by a typical work-hardening behavior to failure. Elevated mechanical testing, performed while the materials were in the austenitic state, revealed yield stresses of approximately 500 MPa and 3.5 pct elongation to failure. Thermal strain recovery characteristics were more carefully investigated with unbiased incremental strain-temperature tests across the 1 to 5 pct strain range, as well as cyclic strain-temperature tests at 3 pct strain. The unbiased shape recovery results indicated a complicated strain recovery path, dependent on prestrain level, but overall acceptable SMA behavior within the targeted temperature and recoverable strain range.
C1 [Buchheit, Thomas E.; Susan, Donald F.; Massad, Jordan E.; Mcelhanon, James R.] Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA.
[Noebe, Ronald D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Buchheit, TE (reprint author), Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA.
EM tebuchh@sandia.gov
FU NASA Transformative Aeronautics Concepts Program (TACP),
Transformational Tools and Technologies Project
FX The authors wish to thank Mark Reece for expertise in arc button
melting. Bonnie McKenzie and Alice Kilgo are acknowledged for SEM work
and metallographic sample preparation. Thanks also to Don Bradley for
DSC analysis, Dave Schmale for expert mechanical testing, and Dereck
Johnson for the ICP analyses. Thanks to Dr. Anita Garg for helpful
discussions and detailed microstructural characterization and Dr. Ken
Eckelmeyer for careful review of the manuscript. RDN would like to
acknowledge additional support from the NASA Transformative Aeronautics
Concepts Program (TACP), Transformational Tools and Technologies
Project.
NR 23
TC 0
Z9 0
U1 1
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1073-5623
EI 1543-1940
J9 METALL MATER TRANS A
JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci.
PD APR
PY 2016
VL 47A
IS 4
BP 1587
EP 1599
DI 10.1007/s11661-016-3324-y
PG 13
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA DF4HA
UT WOS:000371307400011
ER
PT J
AU Rickman, D
Lohn-Wiley, B
Knicely, J
Hannan, B
AF Rickman, Douglas
Lohn-Wiley, Blake
Knicely, Joshua
Hannan, Brian
TI Probabilistic solid form determined from 2D shape measurement
SO POWDER TECHNOLOGY
LA English
DT Article
DE Particle shape; Quantitative; Probability; Stereology, 2D; 3D
ID ROCK PARTICLES; PROJECTED AREA; ROUNDNESS; VOLUME
AB Particle shape, a property of a three-dimensional solid, is an important property. Usually, and problematically, shape measurements of the solid particle are obtained only from two dimensions. It is well known that, in general, a given 2D shape measurement cannot be uniquely related to a solid. However, it is shown herein that unique, and therefore discriminating and useful, probabilistic relationships do exist between a convex solid's shape and 2D measurements taken in either section or projection. The key is to recognize that all possible 2D measurements of a solid make a characteristic probability density surface for an appropriate domain. The measurement domain studied in this paper is often used to measure actual particles. In principle a measured probability density surface of physical samples may be quantitatively approximated by mixtures of model solids. Published by Elsevier B.V.
C1 [Rickman, Douglas; Lohn-Wiley, Blake; Knicely, Joshua; Hannan, Brian] NASA, Earth Sci Off, MSFC, 320 Sparkman Dr, Huntsville, AL 35805 USA.
RP Rickman, D (reprint author), NASA, Earth Sci Off, MSFC, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM drickman@hiwaay.net; blake.lohnwiley@go.Tarleton.edu;
knicely_joshua@yahoo.com; brianmnhannan@gmail.com
OI Rickman, Doug/0000-0003-3409-2882
FU Office of Planetary Protection, National Aeronautics and Space
Administration
FX D. Rickman was funded in part by the Office of Planetary Protection,
National Aeronautics and Space Administration. J. Knicely, B. Lohn-Wiley
and B. Hannan worked as interns at Marshall Space Flight Center and as
volunteers outside of other agreements. The code developed for this work
utilizes the GEOM3D package written by David Legland, of INRA, France,
under the BSC license from the MATLAB Central File Exchange server. The
authors thank Brian Hannan, as a volunteer, for creating an independent
code set to confirm the results of the models. The many discussions with
and encouragement by Alan Rawle of Malvern Instruments is gratefully
acknowledged. Also, the efforts of the three anonymous reviewers greatly
assisted the authors in improving the
NR 26
TC 0
Z9 0
U1 1
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0032-5910
EI 1873-328X
J9 POWDER TECHNOL
JI Powder Technol.
PD APR
PY 2016
VL 291
BP 466
EP 472
DI 10.1016/j.powtec.2015.10.044
PG 7
WC Engineering, Chemical
SC Engineering
GA DE8QH
UT WOS:000370900900049
ER
PT J
AU Kopparla, P
Natraj, V
Spurr, R
Shia, RL
Crisp, D
Yung, YL
AF Kopparla, Pushkar
Natraj, Vijay
Spurr, Robert
Shia, Run-Lie
Crisp, David
Yung, Yuk L.
TI A fast and accurate PCA based radiative transfer model: Extension to the
broadband shortwave region
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Radiative transfer; Principal component analysis; Performance
enhancement; Shortwave broadband; Visible & infrared
ID NONHOMOGENEOUS ATMOSPHERES
AB Accurate radiative transfer (RT) calculations are necessary for many earth-atmosphere applications, from remote sensing retrieval to climate modeling. A Principal Component Analysis (PCA)-based spectral binning method has been shown to provide an order of magnitude increase in computational speed while maintaining an overall accuracy of 0.01% (compared to line-by-line calculations) over narrow spectral bands. In this paper, we have extended the PCA method for RT calculations over the entire shortwave region of the spectrum from 0.3 to 3 microns. The region is divided into 33 spectral fields covering all major gas absorption regimes. We find that the RT performance runtimes are shorter by factors between 10 and 100, while root mean square errors are of order 0.01%. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Kopparla, Pushkar; Shia, Run-Lie; Yung, Yuk L.] CALTECH, Div Geol & Planetaty Sci, MC 150-21, Pasadena, CA 91125 USA.
[Natraj, Vijay; Crisp, David] Jet Prop Lab NASA JPL, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Spurr, Robert] RT Solut Inc, 9 Channing St, Cambridge, MA USA.
RP Kopparla, P (reprint author), CALTECH, Div Geol & Planetaty Sci, MC 150-21, Pasadena, CA 91125 USA.
EM pkk@gps.caltech.edu
FU NASA [NNX13AK34G]; Orbiting Carbon Observatory (OCO-2)
FX We thank members of Prof. Yung's group for useful comments. We also
thank the anonymous referee for insightful suggestions that helped
improve the manuscript. This research was supported in "part by NASA
NNX13AK34G grant to the California Institute of Technology and the
Orbiting Carbon Observatory (OCO-2) Project at JPL.
NR 20
TC 1
Z9 1
U1 1
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2016
VL 173
BP 65
EP 71
DI 10.1016/j.jqsrt.2016.01.014
PG 7
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA DE8ML
UT WOS:000370890000009
ER
PT J
AU Laurila, T
Sainio, S
Jiang, H
Koskinen, J
Koehne, J
Meyyappan, M
AF Laurila, T.
Sainio, S.
Jiang, H.
Koskinen, J.
Koehne, J.
Meyyappan, M.
TI The role of extra carbon source during the pre-annealing stage in the
growth of carbon nanofibers
SO CARBON
LA English
DT Article
ID NANOTUBES; ELECTRODES; CATALYSTS; FILMS
AB In this letter, we discuss the role of a thin diamond-like carbon (DLC) layer in the growth of carbon nanofibers. We show how the DLC layer acts as an additional carbon source during the pre-annealing stage and changes the nanofiber morphology significantly compared to the case without the DLC layer. Significant amount of carbon is dissolved into the Ni layer during the pre-annealing stage, which leads to supersaturation and subsequent precipitation of carbon out of the Ni particles during the growth stage. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Laurila, T.; Sainio, S.] Aalto Univ, Dept Elect Engn & Automat, Sch Elect Engn, Espoo, Finland.
[Jiang, H.] Aalto Univ, Dept Appl Phys, Sch Sci, Espoo, Finland.
[Koskinen, J.] Aalto Univ, Sch Chem Technol, Dept Mat Sci, Espoo, Finland.
[Koehne, J.; Meyyappan, M.] NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Laurila, T (reprint author), Aalto Univ, Dept Elect Engn & Automat, Sch Elect Engn, Espoo, Finland.
EM tomi.laurila@aalto.fi
RI Koskinen, Jari/J-3886-2014; Laurila, Tomi/B-2076-2013
FU Academy of Finland [285015, 285526]
FX The authors T.L. and S.S. acknowledge funding from Academy of Finland
(grant numbers #285015 and #285526). This work made use of the Aalto
University Nanomicroscopy Center facilities.
NR 13
TC 2
Z9 2
U1 2
U2 16
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0008-6223
EI 1873-3891
J9 CARBON
JI Carbon
PD APR
PY 2016
VL 100
BP 351
EP 354
DI 10.1016/j.carbon.2016.01.037
PG 4
WC Chemistry, Physical; Materials Science, Multidisciplinary
SC Chemistry; Materials Science
GA DD5KC
UT WOS:000369961400041
ER
PT J
AU Killen, RM
AF Killen, Rosemary M.
TI Pathways for energization of Ca in Mercury's exosphere
SO ICARUS
LA English
DT Article
DE Terrestrial planets; Mercury; Mercury, atmosphere
ID CALCIUM EXOSPHERE; MESSENGER OBSERVATIONS; IMPACT VAPORIZATION; SPACE
ENVIRONMENT; CLUSTERS; ATMOSPHERES; IONIZATION; SURFACE; PLASMA; ENERGY
AB We investigate the possible pathways to produce the extreme energy observed in the calcium exosphere of Mercury. Any mechanism must explain the facts that Ca in Mercury's exosphere is extremely hot, that it is seen almost exclusively on the dawnside of the planet, and that its content varies seasonally, not sporadically. Simple diatomic molecules or their clusters are considered, focusing on calcium oxides while acknowledging that Ca sulfides may also be the precursor molecules. We first discuss impact vaporization to justify the assumption that CaO and Ca-oxide clusters are expected from impacts on Mercury. Then we discuss processes by which the atomic Ca is energized to a 70,000 K gas. The processes considered are (1) electron-impact dissociation of CaO molecules, (2) spontaneous dissociation of Ca-bearing molecules following impact vaporization, (3) shock-induced dissociative ionization, (4) photodissociation and (5) sputtering. We conclude that electron-impact dissociation cannot produce the required abundance of Ca, and sputtering cannot reproduce the observed spatial and temporal variation that is measured. Spontaneous dissociation is unlikely to result in the high energy that is seen. Of the two remaining processes, shock induced dissociative ionization produces the required energy and comes close to producing the required abundance, but rates are highly dependent on the incoming velocity distribution of the impactors. Photodissociation probably can produce the required abundance of Ca, but simulations show that photodissociation cannot reproduce the observed spatial distribution. Published by Elsevier Inc.
C1 [Killen, Rosemary M.] NASA, Goddard Space Flight Ctr, Magnetospher Phys, Code 695, Greenbelt, MD 20771 USA.
RP Killen, RM (reprint author), NASA, Goddard Space Flight Ctr, Magnetospher Phys, Code 695, Greenbelt, MD 20771 USA.
EM rosemary.killen@nasa.gov
FU NASA Grant [NNX07AR78G]
FX RMK was supported by NASA Grant NNX07AR78G as a Participating Scientist
on the NASA MESSENGER mission to Mercury, by STROFIO, a NASA Mission of
Opportunity on the BepiColombo Mission and by a NASA Discovery Data
Analysis Program grant. RMK thanks Timothy Cassidy and George Ho for a
careful reading of the manuscript.
NR 39
TC 0
Z9 0
U1 1
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2016
VL 268
BP 32
EP 36
DI 10.1016/j.icarus.2015.12.035
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD9AN
UT WOS:000370218100003
ER
PT J
AU Guzewich, SD
Newman, CE
Juarez, MD
Wilson, RJ
Lemmon, M
Smith, MD
Kahanpaa, H
Harri, AM
AF Guzewich, Scott D.
Newman, C. E.
Juarez, M. de la Torre
Wilson, R. J.
Lemmon, M.
Smith, M. D.
Kahanpaa, H.
Harri, A. -M.
CA REMS Sci Team
MSL Sci Team
TI Atmospheric tides in Gale Crater, Mars
SO ICARUS
LA English
DT Article
DE Mars, atmosphere; Atmospheres, dynamics; Meteorology
ID GENERAL-CIRCULATION MODEL; MARTIAN DUST CYCLE; WATER ICE CLOUDS; THERMAL
TIDES; INTERANNUAL VARIABILITY; OPTICAL DEPTH; STORMS; ROVER;
SIMULATION; CLIMATE
AB Atmospheric tides are the primary source of daily air pressure variation at the surface of Mars. These tides are forced by solar heating of the atmosphere and modulated by the presence of atmospheric dust, topography, and surface albedo and thermal inertia. This results in a complex mix of sun-synchronous and non sun-synchronous tides propagating both eastward and westward around the planet in periods that are integer fractions of a solar day. The Rover Environmental Monitoring Station on board the Mars Science Laboratory has observed air pressure at a regular cadence for over 1 Mars year and here we analyze and diagnose atmospheric tides in this pressure record. The diurnal tide amplitude varies from 26 to 63 Pa with an average phase of 0424 local true solar time, while the semidiurnal tide amplitude varies from 5 to 20 Pa with an average phase of 0929. We find that both the diurnal and semidiurnal tides in Gale Crater are highly correlated to atmospheric opacity variations at a value of 0.9 and to each other at a value of 0.77, with some key exceptions occurring during regional and local dust storms. We supplement our analysis with MarsWRF general circulation modeling to examine how a local dust storm impacts the diurnal tide in its vicinity. We find that both the diurnal tide amplitude enhancement and regional coverage of notable amplitude enhancement linearly scales with the size of the local dust storm. Our results provide the first long-term record of surface pressure tides near the martian equator. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Guzewich, Scott D.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA.
[Guzewich, Scott D.; Smith, M. D.] NASA GSFC, Planetary Syst Lab, Greenbelt, MD 20771 USA.
[Guzewich, Scott D.] Univ Space Res Assoc, 7178 Columbia Gateway Dr, Columbia, MD 21046 USA.
[Newman, C. E.] Ashima Res, Pasadena, CA 91106 USA.
[Juarez, M. de la Torre] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Wilson, R. J.] Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA.
[Lemmon, M.] Texas A&M Univ, College Stn, TX 77843 USA.
[Kahanpaa, H.; Harri, A. -M.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Kahanpaa, H.] Aalto Univ, Espoo, Finland.
RP Guzewich, SD (reprint author), Univ Space Res Assoc, 7178 Columbia Gateway Dr, Columbia, MD 21046 USA.
RI Lemmon, Mark/E-9983-2010; Rodriguez-Manfredi, Jose/L-8001-2014;
Gonzalez, Rafael/D-1748-2009; Harri, Ari-Matti/C-7142-2012; Ramos,
Miguel/K-2230-2014;
OI Lemmon, Mark/0000-0002-4504-5136; Rodriguez-Manfredi,
Jose/0000-0003-0461-9815; Harri, Ari-Matti/0000-0001-8541-2802; Ramos,
Miguel/0000-0003-3648-6818; Guzewich, Scott/0000-0003-1149-7385
FU MSL Participating Scientist grant; MSL mission
FX This work was partially funded by a MSL Participating Scientist grant to
M.D. Smith. C.E. Newman, M. de la Torre Juarez, and M. Lemmon
acknowledge funding from the MSL mission, the REMS team, and the MastCam
team. MarsWRF simulations were conducted on the NASA Pleiades Advanced
Supercomputer system.
NR 46
TC 1
Z9 1
U1 4
U2 22
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2016
VL 268
BP 37
EP 49
DI 10.1016/j.icarus.2015.12.028
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD9AN
UT WOS:000370218100004
ER
PT J
AU Thomas, PC
Calvin, W
Cantor, B
Haberle, R
James, PB
Lee, SW
AF Thomas, P. C.
Calvin, W.
Cantor, B.
Haberle, R.
James, P. B.
Lee, S. W.
TI Mass balance of Mars' residual south polar cap from CTX images and other
data
SO ICARUS
LA English
DT Article
DE Mars, climate; Mars, polar caps; Mars, atmosphere; Mars
ID INTERANNUAL VARIABILITY; CARBON-DIOXIDE; DUST STORM; ICE; VIKING;
DEPOSITION; MODELS; DEPTH
AB Erosion of pits in the residual south polar cap (RSPC) of Mars concurrent with deposition and fluctuating cap boundaries raises questions about the mass balance and long term stability of the cap. Determining a mass balance by measurement of a net gain or loss of atmospheric CO2 by direct pressure measurements (Haberle, R.M. et al. [2014]. Secular climate change on Mars: An update using one Mars year of MSL pressure data. American Geophysical Union (Fall). Abstract 3947), although perhaps the most direct method, has so far given ambiguous results. Estimating volume changes from imaging data faces challenges, and has previously been attempted only in isolated areas of the cap. In this study we use 6 m/pixel Context Imager (CTX) data from Mars year 31 to map all the morphologic units of the RSPC, expand the measurement record of pit erosion rates, and use high resolution images to place limits on vertical changes in the surface of the residual cap. We find the mass balance in Mars years 9-31 to be -6 to +4 ke/male y, or roughly--0.039% to +0.026% of the mean atmospheric CO2 mass/male y. The indeterminate sign results chiefly from uncertainty in the amounts of deposition or erosion on the upper surfaces of deposits (as opposed to scarp retreat). Erosion and net deposition in this period appear to be controlled by summertime planetary scale dust events, the largest occurring in MY 9, another, smaller one in MY 28. The rates of erosion and the deposition observed since MY 9 appear to be consistent with the types of deposits and erosional behavior found in most of the residual cap. However, small areas (<10%) of the cap are distinguished by their greater thickness, polygonal troughs, and embayed contacts with thinner units. These deposits may require extended periods (>100 male y) of depositional and/or erosional conditions different from those occurring in the period since MY 9, although these environmental differences could be subtle. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Thomas, P. C.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
[Calvin, W.] Univ Nevada, Dept Geol Sci, Reno, NV 89577 USA.
[Cantor, B.] Malin Space Sci Syst, San Diego, CA 92191 USA.
[Haberle, R.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[James, P. B.] Space Sci Inst, Boulder, CO 80301 USA.
[Lee, S. W.] Denver Museum Nat & Sci, 2001 Colorado Blvd, Denver, CO 80205 USA.
RP Thomas, PC (reprint author), Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
NR 46
TC 2
Z9 2
U1 4
U2 9
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2016
VL 268
BP 118
EP 130
DI 10.1016/j.icarus.2015.12.038
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD9AN
UT WOS:000370218100010
ER
PT J
AU Stallard, TS
Clarke, JT
Melin, H
Miller, S
Nichols, JD
O'Donoghue, J
Johnson, RE
Connerney, JEP
Satoh, T
Perry, M
AF Stallard, Tom S.
Clarke, John T.
Melin, Henrik
Miller, Steve
Nichols, Jon D.
O'Donoghue, James
Johnson, Rosie E.
Connerney, John E. P.
Satoh, Takehiko
Perry, Michael
TI Stability within Jupiter's polar auroral 'Swirl region' over moderate
timescales
SO ICARUS
LA English
DT Article
DE Aurorae; Jupiter, atmosphere; Infrared observations; Ionospheres
ID INFRARED TELESCOPE FACILITY; EMISSION; ULTRAVIOLET; IONOSPHERE; IO;
THERMOSPHERE; ATMOSPHERE; MODEL; OVAL
AB Jupiter's Swirl region, poleward of the main auroral emission, has been characterised in previous observations as having highly variable auroral emission, changing dramatically across the region on a two minute timescale, the typical integration time for UV images. This variability has made comparisons with H-3(+) emission difficult. Here, we show that the Swirl region in H-3(+) images is characterised by relatively stable emission, often with an arc of emission on the boundary between the Swirl and Dark regions. Coadding multiple UV images taken over the approximate lifetime of the H-3(+) molecule in the ionosphere, show similar structures to those observed in the H-3(+) images. Our analysis shows that UV auroral morphology within Jupiter's Swirl region is only highly variable on short timescales of similar to 100 s, an intrinsic property of the particle precipitation process, but this variability drops away on timescales of 5-15 min. On moderate timescales between 10 and 100 min, the Swirl region is stable, evolving through as yet unknown underlying magnetospheric interactions. This shows that observing the UV aurora over time scales 5-15 min resolves clear auroral structures that will help us understand the magnetospheric origin of these features, and that calculating the variability over different timescales, especially >15 min, provides a new and important new tool in our understanding of Jupiter's polar aurora. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Stallard, Tom S.; Melin, Henrik; Nichols, Jon D.; Johnson, Rosie E.; Perry, Michael] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
[Clarke, John T.; O'Donoghue, James] Boston Univ, Ctr Space Phys, 725 Commonwealth Ave, Boston, MA 02215 USA.
[Miller, Steve] UCL, Dept Phys & Astron, Astrophys Grp, Gower St, London WC1E 6BT, England.
[Connerney, John E. P.] NASA, Goddard Space Flight Ctr, Mail Code 695, Greenbelt, MD 20771 USA.
[Satoh, Takehiko] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Yoshinodai 3-1-1, Sagamihara, Kanagawa 2525210, Japan.
RP Stallard, TS (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.
EM tss8@leicester.ac.uk
RI Clarke, John/C-8644-2013; Nichols, Jonathan/F-5764-2010;
OI Nichols, Jonathan/0000-0002-8004-6409; Stallard, Tom/0000-0003-3990-670X
FU UK STFC; National Aeronautics and Space Administration, Science Mission
Directorate, Planetary Astronomy Program [NNX-08AE38A]
FX This work was supported by the UK STFC for H.M., T.S. and J.N., and with
a PhD studentship for R.J. Undergraduates. This analysis came about
following discussions within the ISSI Team Nichols and Team Stallard
workshops. J.E.P. Connerney and Takehiko Satoh were visiting astronomers
at the NASA Infrared Telescope Facility, which is operated by the
University of Hawaii under Cooperative Agreement No. NNX-08AE38A with
the National Aeronautics and Space Administration, Science Mission
Directorate, Planetary Astronomy Program. Infrared data is available
from the Magnetospheres of the Outer Planets Infrared Data Archive.
Ultraviolet data is available from Hubble Legacy Archive.
NR 36
TC 2
Z9 2
U1 0
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2016
VL 268
BP 145
EP 155
DI 10.1016/j.icarus.2015.12.044
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD9AN
UT WOS:000370218100012
ER
PT J
AU Barth, EL
Farrell, WM
Rafkin, SCR
AF Barth, Erika L.
Farrell, William M.
Rafkin, Scot C. R.
TI Electric field generation in martian dust devils
SO ICARUS
LA English
DT Article
DE Mars, atmosphere; Mars, surface; Aeolian processes
ID MARS PATHFINDER; ELECTROSTATIC DISCHARGES; OXIDANT ENHANCEMENT; STORMS;
SIMULATIONS; CONVECTION; MODEL; ELECTRIFICATION; THUNDERSTORM;
ATMOSPHERES
AB Terrestrial dust devils are known to generate electric fields from the vertical separation of charged dust particles. The particles present within the dust devils on Mars may also be subject to similar charging processes and so likely contribute to electric field generation there as well. However, to date, no Mars in situ instrumentation has been deployed to measure electric field strength. In order to explore the electric environment of dust devils on Mars, the triboelectric dust charging physics from the Macroscopic Triboelectric Simulation (MTS) code has been coupled to the Mars Regional Atmospheric Modeling System (MRAMS). Using this model, we examine how macroscopic electric fields are generated within martian dust disturbances and attempt to quantify the time evolution of the electrodynamical system. Electric fields peak for several minutes within the dust devil simulations. The magnitude of the electric field is a strong function of the size of the particles present, the average charge on the particles and the number of particles lifted. Varying these parameters results in peak electric fields between tens of millivolts per meter and tens of kilovolts per meter. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Barth, Erika L.; Rafkin, Scot C. R.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Farrell, William M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
RP Barth, EL (reprint author), SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
EM ebarth@boulder.swri.edu
RI Farrell, William/I-4865-2013
FU Mars Fundamental Research Program, NASA [NNX07AR69G]
FX This research was supported by the Mars Fundamental Research Program,
NASA Grant NNX07AR69G. We also thank Tim Michaels for many useful
discussions regarding dust devil modeling with the MRAMS code.
NR 65
TC 3
Z9 3
U1 5
U2 19
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2016
VL 268
BP 253
EP 265
DI 10.1016/j.icarus.2015.12.020
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD9AN
UT WOS:000370218100018
ER
PT J
AU Pajola, M
Rossato, S
Baratti, E
Mangili, C
Mancarella, F
McBride, K
Coradini, M
AF Pajola, Maurizio
Rossato, Sandro
Baratti, Emanuele
Mangili, Clara
Mancarella, Francesca
McBride, Karen
Coradini, Marcello
TI The Simud-Tiu Valles hydrologic system: A multidisciplinary study of a
possible site for future Mars on-site exploration
SO ICARUS
LA English
DT Article
DE Mars; Mars, surface; Geological processes; Image processing; Mineralogy;
Exobiology
ID EMISSION SPECTROMETER EXPERIMENT; SIZE-FREQUENCY DISTRIBUTIONS; ORBITER
LASER ALTIMETER; REFLECTANCE SPECTROSCOPY; GLOBAL SURVEYOR; RESURFACING
HISTORY; PHYSICAL-PROPERTIES; OMEGA/MARS EXPRESS; MARTIAN CHANNELS;
SULFATE MINERALS
AB When looking for traces of past life on Mars, we have to look primarily for places where water was present, possibly for long time intervals. The Simud and Tiu Valles are two large outflow channels connected to the north with the Chryse Basin, Oxia Palus quadrangle. The area, carved by water during the Noachian/Early Hesperian is characterized by a complex geological evolution. The geomorphological analysis shows the presence of fluvial and alluvial structures, interpreted as fluvial channels and terraces, debris flow fronts and short-lasting small water flows coexisting with maar-diatremes and mud volcanoes. Several morphological features indicate a change in water flux direction after the main erosive phase. During this period water originated from the Masursky crater and flown southwards into the Hydraotes Chaos. This phenomenon caused the studied area to become a depocenter where fine-grained material deposition took place, possibly in association with ponding water. This setting is potentially quite valuable as traces of life may have been preserved. The presence of water at various times over a period of about 1 Ga in the area is corroborated by mineralogical analyses of different areas that indicate the possible presence of hydrated minerals mixtures, such as sulfate-bearing deposits. Given the uniqueness of the evolution of this region, the long term interactions between fluvial, volcanic, and tectonic processes and its extremely favorable landing parameters (elevation, slope, roughness, rock distribution, thermal inertia, albedo, etc.), we decided to propose this location as a possible landing site for the ESA ExoMars 2018, the NASA Mars 2020 and future on-site missions. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Pajola, Maurizio] Univ Padua, Ctr Studies & Activ Space G Colombo, Via Venezia 15, I-35131 Padua, Italy.
[Pajola, Maurizio] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rossato, Sandro] Univ Padua, Dept Geosci, Padua, Italy.
[Baratti, Emanuele] Univ Bologna, Sch Civil Engn, Dept DICAM, Bologna, Italy.
[Mangili, Clara] Univ Geneva, Earth & Environm Sci, Geneva, Switzerland.
[Mancarella, Francesca] Univ Salento, Dept Math & Phys E De Giorgi, Lecce, Italy.
[McBride, Karen] Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
[Coradini, Marcello] European Space Agcy, Paris, France.
[Coradini, Marcello] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Pajola, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM maurizio.pajola@gmail.com
RI Rossato, Sandro/R-2353-2016;
OI Rossato, Sandro/0000-0002-1075-2586; Pajola,
Maurizio/0000-0002-3144-1277; Coradini, Marcello/0000-0002-1711-3197
FU NASA Postdoctoral Program at Ames Research Center
FX We would like to thank Dr. Giuseppe Galletta and Dr. Gianni Tamino for
the important interaction and discussions about the Exobiology relevance
of the proposed site. This research was supported in part by an
appointment to the NASA Postdoctoral Program at Ames Research Center,
administered by Oak Ridge Associated Universities through a contract
with NASA.
NR 127
TC 1
Z9 1
U1 6
U2 16
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2016
VL 268
BP 355
EP 381
DI 10.1016/j.icarus.2015.12.049
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DD9AN
UT WOS:000370218100024
ER
PT J
AU Nouri, N
Panerai, F
Tagavi, KA
Mansour, NN
Martin, A
AF Nouri, Nima
Panerai, Francesco
Tagavi, Kaveh A.
Mansour, Nagi N.
Martin, Alexandre
TI Evaluation of the anisotropic radiative conductivity of a low-density
carbon fiber material from realistic microscale imaging
SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER
LA English
DT Article
DE Radiative heat transfer; Porous media; Radiative conductivity; Effective
conductivity; Thermal Protection Systems
ID HEAT-TRANSFER MODEL; VALIDATION
AB The radiative heat transfer inside a low-density carbon fiber insulator is analyzed using a three-dimensional direct simulation model. A robust procedure is presented for the numerical calculation of the geometric configuration factor to compute the radiative energy exchange processes among the small discretized surface areas of the fibrous material. The methodology is applied to a polygonal mesh of a fibrous insulator obtained from three-dimensional microscale imaging of the real material. The anisotropic values of the radiative conductivity are calculated for that geometry. The results yield both directional and thermal dependence of the radiative conductivity. The combined value of radiative and solid conductivity are compared to experimental data available in the literature, and show excellent agreement. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Nouri, Nima; Panerai, Francesco; Tagavi, Kaveh A.; Martin, Alexandre] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Martin, Alexandre] Univ Kentucky, Ctr Computat Sci, Lexington, KY 40506 USA.
[Nouri, Nima] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA.
[Mansour, Nagi N.] NASA, Ames Res Ctr, NASA Adv Supercomp NAS Div, Moffett Field, CA 94035 USA.
RP Martin, A (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
EM Nima.Nouri@uky.edu; Francesco.Panerai@uky.edu; Kaveh.Tagavi@uky.edu;
Nagi.N.Mansour@nasa.gov; Alexandre.Martin@uky.edu
OI Martin, Alexandre/0000-0003-2216-2468
FU Kentucky EPSCoR; NASA RA Award [NNX13AN04A]; NASA [NNX14AI97G]
FX The authors gratefully acknowledge the support of B. Plaster regarding
this work. Financial support was provided by Kentucky EPSCoR and NASA RA
Award NNX13AN04A and NASA Award NNX14AI97G. Part of this work was also
performed under the Entry System Modeling Project (M.J. Wright program
manager) of the NASA Game Changing Development (GCD) Program. Finally,
the authors are also indebted to T. Cochell for pointing out the
published experimental data, K. Bensassi and A. Munafo for providing
helpful comments, and J.F. Wenk for a very helpful conversation on
principal axis.
NR 19
TC 0
Z9 0
U1 2
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0017-9310
EI 1879-2189
J9 INT J HEAT MASS TRAN
JI Int. J. Heat Mass Transf.
PD APR
PY 2016
VL 95
BP 535
EP 539
DI 10.1016/j.ijheatmasstransfer.2015.12.004
PG 5
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA DD7NK
UT WOS:000370111200049
ER
PT J
AU Nguyen, TTT
Kundan, A
Wayner, PC
Plawsky, JL
Chao, DF
Sicker, RJ
AF Nguyen, Thao T. T.
Kundan, Akshay
Wayner, Peter C., Jr.
Plawsky, Joel L.
Chao, David F.
Sicker, Ronald J.
TI The effect of an ideal fluid mixture on the evaporator performance of a
heat pipe in microgravity
SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER
LA English
DT Article
DE Ideal liquid mixture; Marangoni stress; Interfacial heat transfer;
Capillarity; Heat pipe
ID VAPOR BUBBLE EXPERIMENT; CONTACT LINE REGION; BINARY-MIXTURES;
THIN-FILM; CAPILLARY; ANGLES; WEDGE; FABRICATION; MENISCUS; SURFACE
AB Previous studies on wickless heat pipes showed that a temperature induced "Marangoni flow" prevents liquid from recirculating to the heater end, and therefore reduces the effectiveness of the heat pipe. Recently, several research groups used a water and alcohol mixture, with a low concentration of alcohol, resulting in better performance of the heat pipe. The alcohol/water combinations were peculiar in that for a certain composition range, the surface tension increases with increasing temperature thereby driving liquid toward the hotter end. It was believed that changing the direction of the Marangoni stress or reducing its magnitude by differential evaporation of an ideal binary mixture would also improve the performance of the heat pipe. For the first time, an ideal fluid mixture of 94 vol%-pentane and 6 vol%-isohexane was used as the working fluid in the Constrained Vapor Bubble (CVB) heat pipe experiment on the International Space Station (ISS). Using a simple heat transfer model developed in our laboratory, an internal heat transfer coefficient in the evaporator section was determined and shown to be almost twice that of the case where pure pentane was used under the same conditions. The Marangoni stress in the mixture was five times lower. Interestingly, reducing the Marangoni stress led to less liquid accumulation near the heater end and surveillance images of the device, taken at the steady state, showed that the bubble gets much closer to the heater end in the mixture case instead of being isolated from the heater by a thick liquid pool as in the pure pentane case. The proximity of the bubble to the heater wall led to more evaporation at the heater end in the mixture case, and therefore a higher heat transfer coefficient. The pressure profile calculated from the Young-Laplace equation supports the observations made from the surveillance images. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Nguyen, Thao T. T.; Kundan, Akshay; Wayner, Peter C., Jr.; Plawsky, Joel L.] Rensselaer Polytech Inst, Howard P Isermann Dept Chem & Biol Engn, Troy, NY 12180 USA.
[Chao, David F.; Sicker, Ronald J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Plawsky, JL (reprint author), Rensselaer Polytech Inst, Howard P Isermann Dept Chem & Biol Engn, Troy, NY 12180 USA.
EM nguyen.thaoche@gmail.com; akshaykundan@gmail.com; wayner@rpi.edu;
plawsky@rpi.edu; david.f.chao@nasa.gov; ronald.j.sicker@nasa.gov
FU National Aeronautics and Space Administration [NNX13AQ78G]
FX This material is based on the work supported by the National Aeronautics
and Space Administration under Grant number NNX13AQ78G. Any opinions,
findings, and conclusions or recommendations expressed in this
publication are those of the authors and do not necessarily reflect the
view of NASA.
NR 53
TC 2
Z9 2
U1 4
U2 14
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0017-9310
EI 1879-2189
J9 INT J HEAT MASS TRAN
JI Int. J. Heat Mass Transf.
PD APR
PY 2016
VL 95
BP 765
EP 772
DI 10.1016/j.ijheatmasstransfer.2015.12.032
PG 8
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA DD7NK
UT WOS:000370111200070
ER
PT J
AU Gu, QJ
Li, JC
Tang, A
AF Gu, Qun Jane
Li, James C.
Tang, Adrian
TI Power detectors for integrated microwave/mm-wave imaging systems in
mainstream silicon technologies
SO SOLID-STATE ELECTRONICS
LA English
DT Article
DE Bipolar; CMOS; Detector; Imager; Super-regenerative
ID NM CMOS; TRANSCEIVER; RECEIVER; GHZ
AB This paper analyzes and compares three different types of detectors, including CMOS power detectors, bipolar power detectors, and super-regenerative detectors, deployed in the literature for integrated microwave/mm-wave imaging systems in mainstream silicon technologies. Each detector has unique working mechanism and demonstrates different behavior with respects to bias conditions, input signal power, as well as bandwidth responses. Two Figure-of-Merits for both wideband and narrowband imaging have been defined to quantify the detector performance comparison. CMOS and Bipolar detectors are good for passive imaging, while super regenerative detectors are superior for active imaging. The analytical results have been verified by both simulation and measurement results. These analyses intend to provide design insights and guidance for integrated microwave/ mm-wave imaging power detectors. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Gu, Qun Jane] Univ Calif Davis, Davis, CA USA.
[Li, James C.] HRL Labs LLC, Malibu, CA 90265 USA.
[Tang, Adrian] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Gu, QJ (reprint author), Univ Calif Davis, Davis, CA USA.
EM jgu@ucdavis.edu; jli@hrl.com; Adrian.J.Tang@jpl.nasa.gov
FU DARPA COSMOS Program
FX The authors would like to thank DARPA COSMOS Program and Dr. Sanjay
Raman for funding support.
NR 25
TC 0
Z9 0
U1 5
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0038-1101
EI 1879-2405
J9 SOLID STATE ELECTRON
JI Solid-State Electron.
PD APR
PY 2016
VL 118
BP 46
EP 55
DI 10.1016/j.sse.2016.01.008
PG 10
WC Engineering, Electrical & Electronic; Physics, Applied; Physics,
Condensed Matter
SC Engineering; Physics
GA DD3OH
UT WOS:000369831300009
ER
PT J
AU Abbott, BP
Abbott, R
Abbott, TD
Abernathy, MR
Acernese, F
Ackley, K
Adams, C
Adams, T
Addesso, P
Adhikari, RX
Adya, VB
Affeldt, C
Agathos, M
Agatsuma, K
Aggarwal, N
Aguiar, OD
Aiello, L
Ain, A
Ajith, P
Allen, B
Allocca, A
Altin, PA
Anderson, SB
Anderson, WG
Arai, K
Araya, MC
Arceneaux, CC
Areeda, JS
Arnaud, N
Arun, KG
Ascenzi, S
Ashton, G
Ast, M
Aston, SM
Astone, P
Aufmuth, P
Aulbert, C
Babak, S
Bacon, P
Bader, MKM
Baker, PT
Baldaccini, F
Ballardin, G
Ballmer, SW
Barayoga, JC
Barclay, SE
Barish, BC
Barker, D
Barone, F
Barr, B
Barsotti, L
Barsuglia, M
Barta, D
Bartlett, J
Bartos, I
Bassiri, R
Basti, A
Batch, JC
Baune, C
Bavigadda, V
Bazzan, M
Behnke, B
Bejger, M
Bell, AS
Bell, CJ
Berger, BK
Bergman, J
Bergmann, G
Berry, CPL
Bersanetti, D
Bertolini, A
Betzwieser, J
Bhagwat, S
Bhandare, R
Bilenko, IA
Billingsley, G
Birch, J
Birney, R
Biscans, S
Bisht, A
Bitossi, M
Biwer, C
Bizouard, MA
Blackburn, JK
Blair, CD
Blair, DG
Blair, RM
Bloemen, S
Bock, O
Bodiya, TP
Boer, M
Bogaert, G
Bogan, C
Bohe, A
Bojtos, P
Bond, C
Bondu, F
Bonnand, R
Boom, BA
Bork, R
Boschi, V
Bose, S
Bouffanais, Y
Bozzi, A
Bradaschia, C
Brady, PR
Braginsky, VB
Branchesi, M
Brau, JE
Briant, T
Brillet, A
Brinkmann, M
Brisson, V
Brockill, P
Brooks, AF
Brown, DA
Brown, DD
Brown, NM
Buchanan, CC
Buikema, A
Bulik, T
Bulten, HJ
Buonanno, A
Buskulic, D
Buy, C
Byer, RL
Cadonati, L
Cagnoli, G
Cahillane, C
Bustillo, JC
Callister, T
Calloni, E
Camp, JB
Cannon, KC
Cao, J
Capano, CD
Capocasa, E
Carbognani, F
Caride, S
Diaz, JC
Casentini, C
Caudill, S
Cavaglia, M
Cavalier, F
Cavalieri, R
Cella, G
Cepeda, CB
Baiardi, LC
Cerretani, G
Cesarini, E
Chakraborty, R
Chalermsongsak, T
Chamberlin, SJ
Chan, M
Chao, S
Charlton, P
Chassande-Mottin, E
Chen, HY
Chen, Y
Cheng, C
Chincarini, A
Chiummo, A
Cho, HS
Cho, M
Chow, JH
Christensen, N
Chu, Q
Chua, S
Chung, S
Ciani, G
Clara, F
Clark, JA
Cleva, F
Coccia, E
Cohadon, PF
Colla, A
Collette, CG
Cominsky, L
Constancio, M
Conte, A
Conti, L
Cook, D
Corbitt, TR
Cornish, N
Corsi, A
Cortese, S
Costa, CA
Coughlin, MW
Coughlin, SB
Coulon, JP
Countryman, ST
Couvares, P
Cowan, EE
Coward, DM
Cowart, MJ
Coyne, DC
Coyne, R
Craig, K
Creighton, JDE
Cripe, J
Crowder, SG
Cumming, A
Cunningham, L
Cuoco, E
Dal Canton, T
Danilishin, SL
D'Antonio, S
Danzmann, K
Darman, NS
Dattilo, V
Dave, I
Daveloza, HP
Davier, M
Davies, GS
Daw, EJ
Day, R
DeBra, D
Debreczeni, G
Degallaix, J
De Laurentis, M
Deleglise, S
Del Pozzo, W
Denker, T
Dent, T
Dereli, H
Dergachev, V
DeRosa, RT
De Rosa, R
DeSalvo, R
Dhurandhar, S
Diaz, MC
Di Fiore, L
Di Giovanni, M
Di Lieto, A
Di Pace, S
Di Palma, I
Di Virgilio, A
Dojcinoski, G
Dolique, V
Donovan, F
Dooley, KL
Doravari, S
Douglas, R
Downes, TP
Drago, M
Drever, RWP
Driggers, JC
Du, Z
Ducrot, M
Dwyer, SE
Edo, TB
Edwards, MC
Effler, A
Eggenstein, HB
Ehrens, P
Eichholz, J
Eikenberry, SS
Engels, W
Essick, RC
Etzel, T
Evans, M
Evans, TM
Everett, R
Factourovich, M
Fafone, V
Fair, H
Fairhurst, S
Fan, X
Fang, Q
Farinon, S
Farr, B
Farr, WM
Favata, M
Fays, M
Fehrmann, H
Fejer, MM
Ferrante, I
Ferreira, EC
Ferrini, F
Fidecaro, F
Fiori, I
Fiorucci, D
Fisher, RP
Flaminio, R
Fletcher, M
Fournier, JD
Franco, S
Frasca, S
Frasconi, F
Frei, Z
Freise, A
Frey, R
Frey, V
Fricke, TT
Fritschel, P
Frolov, VV
Fulda, P
Fyffe, M
Gabbard, HAG
Gair, JR
Gammaitoni, L
Gaonkar, SG
Garufi, F
Gatto, A
Gaur, G
Gehrels, N
Gemme, G
Gendre, B
Genin, E
Gennai, A
George, J
Gergely, L
Germain, V
Ghosh, A
Ghosh, S
Giaime, JA
Giardina, KD
Giazotto, A
Gill, K
Glaefke, A
Goetz, E
Goetz, R
Gondan, L
Gonzalez, G
Castro, JMG
Gopakumar, A
Gordon, NA
Gorodetsky, ML
Gossan, SE
Gosselin, M
Gouaty, R
Graef, C
Graff, PB
Granata, M
Grant, A
Gras, S
Gray, C
Greco, G
Green, AC
Groot, P
Grote, H
Grunewald, S
Guidi, GM
Guo, X
Gupta, A
Gupta, MK
Gushwa, KE
Gustafson, EK
Gustafson, R
Hacker, JJ
Hall, BR
Hall, ED
Hammond, G
Haney, M
Hanke, MM
Hanks, J
Hanna, C
Hannam, MD
Hanson, J
Hardwick, T
Haris, K
Harms, J
Harry, GM
Harry, IW
Hart, MJ
Hartman, MT
Haster, CJ
Haughian, K
Heidmann, A
Heintze, MC
Heitmann, H
Hello, P
Hemming, G
Hendry, M
Heng, IS
Hennig, J
Heptonstall, AW
Heurs, M
Hild, S
Hoak, D
Hodge, KA
Hofman, D
Hollitt, SE
Holt, K
Holz, DE
Hopkins, P
Hosken, DJ
Hough, J
Houston, EA
Howell, EJ
Hu, YM
Huang, S
Huerta, EA
Huet, D
Hughey, B
Husa, S
Huttner, SH
Huynh-Dinh, T
Idrisy, A
Indik, N
Ingram, DR
Inta, R
Isa, HN
Isac, JM
Isi, M
Islas, G
Isogai, T
Iyer, BR
Izumi, K
Jacqmin, T
Jang, H
Jani, K
Jaranowski, P
Jawahar, S
Jimenez-Forteza, F
Johnson, WW
Jones, DI
Jones, R
Jonker, RJG
Ju, L
Kalaghatgi, CV
Kalogera, V
Kandhasamy, S
Kang, G
Kanner, JB
Karki, S
Kasprzack, M
Katsavounidis, E
Katzman, W
Kaufer, S
Kaur, T
Kawabe, K
Kawazoe, F
Kefelian, F
Kehl, MS
Keitel, D
Kelley, DB
Kells, W
Kennedy, R
Key, JS
Khalaidovski, A
Khalili, FY
Khan, I
Khan, S
Khan, Z
Khazanov, EA
Kijbunchoo, N
Kim, C
Kim, J
Kim, K
Kim, NG
Kim, N
Kim, YM
King, EJ
King, PJ
Kinzel, DL
Kissel, JS
Kleybolte, L
Klimenko, S
Koehlenbeck, SM
Kokeyama, K
Koley, S
Kondrashov, V
Kontos, A
Korobko, M
Korth, WZ
Kowalska, I
Kozak, DB
Kringel, V
Krolak, A
Krueger, C
Kuehn, G
Kumar, P
Kuo, L
Kutynia, A
Lackey, BD
Landry, M
Lange, J
Lantz, B
Lasky, PD
Lazzarini, A
Lazzaro, C
Leaci, P
Leavey, S
Lebigot, EO
Lee, CH
Lee, HK
Lee, HM
Lee, K
Lenon, A
Leonardi, M
Leong, JR
Leroy, N
Letendre, N
Levin, Y
Levine, BM
Li, TGF
Libson, A
Littenberg, TB
Lockerbie, NA
Logue, J
Lombardi, AL
Lord, JE
Lorenzini, M
Loriette, V
Lormand, M
Losurdo, G
Lough, JD
Lueck, H
Lundgren, AP
Luo, J
Lynch, R
Ma, Y
MacDonald, T
Machenschalk, B
MacInnis, M
Macleod, DM
Magana-Sandoval, F
Magee, RM
Mageswaran, M
Majorana, E
Maksimovic, I
Malvezzi, V
Man, N
Mandel, I
Mandic, V
Mangano, V
Mansell, GL
Manske, M
Mantovani, M
Marchesoni, F
Marion, F
Marka, S
Marka, Z
Markosyan, AS
Maros, E
Martelli, F
Martellini, L
Martin, IW
Martin, RM
Martynov, DV
Marx, JN
Mason, K
Masserot, A
Massinger, TJ
Masso-Reid, M
Matichard, F
Matone, L
Mavalvala, N
Mazumder, N
Mazzolo, G
McCarthy, R
McClelland, DE
McCormick, S
McGuire, SC
McIntyre, G
McIver, J
McManus, DJ
McWilliams, ST
Meacher, D
Meadors, GD
Meidam, J
Melatos, A
Mendell, G
Mendoza-Gandara, D
Mercer, RA
Merilh, E
Merzougui, M
Meshkov, S
Messenger, C
Messick, C
Meyers, PM
Mezzani, F
Miao, H
Michel, C
Middleton, H
Mikhailov, EE
Milano, L
Miller, J
Millhouse, M
Minenkov, Y
Ming, J
Mirshekari, S
Mishra, C
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Moggi, A
Mohan, M
Mohapatra, SRP
Montani, M
Moore, BC
Moore, CJ
Moraru, D
Moreno, G
Morriss, SR
Mossavi, K
Mours, B
Mow-Lowry, CM
Mueller, CL
Mueller, G
Muir, AW
Mukherjee, A
Mukherjee, D
Mukherjee, S
Mukund, N
Mullavey, A
Munch, J
Murphy, DJ
Murray, PG
Mytidis, A
Nardecchia, I
Naticchioni, L
Nayak, RK
Necula, V
Nedkova, K
Nelemans, G
Neri, M
Neunzert, A
Newton, G
Nguyen, TT
Nielsen, AB
Nissanke, S
Nitz, A
Nocera, F
Nolting, D
Normandin, ME
Nuttall, LK
Oberling, J
Ochsner, E
O'Dell, J
Oelker, E
Ogin, GH
Oh, JJ
Oh, SH
Ohme, F
Oliver, M
Oppermann, P
Oram, RJ
O'Reilly, B
O'Shaughnessy, R
Ottaway, DJ
Ottens, RS
Overmier, H
Owen, BJ
Pai, A
Pai, SA
Palamos, JR
Palashov, O
Palomba, C
Pal-Singh, A
Pan, H
Pankow, C
Pannarale, F
Pant, BC
Paoletti, F
Paoli, A
Papa, MA
Paris, HR
Parker, W
Pascucci, D
Pasqualetti, A
Passaquieti, R
Passuello, D
Patricelli, B
Patrick, Z
Pearlstone, BL
Pedraza, M
Pedurand, R
Pekowsky, L
Pele, A
Penn, S
Perreca, A
Phelps, M
Piccinni, O
Pichot, M
Piergiovanni, F
Pierro, V
Pillant, G
Pinard, L
Pinto, IM
Pitkin, M
Poggiani, R
Popolizio, P
Post, A
Powell, J
Prasad, J
Predoi, V
Premachandra, SS
Prestegard, T
Price, LR
Prijatelj, M
Principe, M
Privitera, S
Prodi, GA
Prokhorov, L
Puncken, O
Punturo, M
Puppo, P
Puerrer, M
Qi, H
Qin, J
Quetschke, V
Quintero, EA
Quitzow-James, R
Raab, FJ
Rabeling, DS
Radkins, H
Raffai, P
Raja, S
Rakhmanov, M
Rapagnani, P
Raymond, V
Razzano, M
Re, V
Read, J
Reed, CM
Regimbau, T
Rei, L
Reid, S
Reitze, DH
Rew, H
Reyes, SD
Ricci, F
Riles, K
Robertson, NA
Robie, R
Robinet, F
Rocchi, A
Rolland, L
Rollins, JG
Roma, VJ
Romano, R
Romanov, G
Romie, JH
Rosinska, D
Rowan, S
Rudiger, A
Ruggi, P
Ryan, K
Sachdev, S
Sadecki, T
Sadeghian, L
Salconi, L
Saleem, M
Salemi, F
Samajdar, A
Sammut, L
Sanchez, EJ
Sandberg, V
Sandeen, B
Sanders, JR
Sassolas, B
Sathyaprakash, BS
Saulson, PR
Sauter, O
Savage, RL
Sawadsky, A
Schale, P
Schilling, R
Schmidt, J
Schmidt, P
Schnabel, R
Schofield, RMS
Schonbeck, A
Schreiber, E
Schuette, D
Schutz, BF
Scott, J
Scott, SM
Sellers, D
Sengupta, AS
Sentenac, D
Sequino, V
Sergeev, A
Serna, G
Setyawati, Y
Sevigny, A
Shaddock, DA
Shah, S
Shahriar, MS
Shaltev, M
Shao, Z
Shapiro, B
Shawhan, P
Sheperd, A
Shoemaker, DH
Shoemaker, DM
Siellez, K
Siemens, X
Sigg, D
Silva, AD
Simakov, D
Singer, A
Singer, LP
Singh, A
Singh, R
Singhal, A
Sintes, AM
Slagmolen, BJJ
Smith, JR
Smith, ND
Smith, RJE
Son, EJ
Sorazu, B
Sorrentino, F
Souradeep, T
Srivastava, AK
Staley, A
Steinke, M
Steinlechner, J
Steinlechner, S
Steinmeyer, D
Stephens, BC
Stone, R
Strain, KA
Straniero, N
Stratta, G
Strauss, NA
Strigin, S
Sturani, R
Stuver, AL
Summerscales, TZ
Sun, L
Sutton, PJ
Swinkels, BL
Szczepanczyk, MJ
Tacca, M
Talukder, D
Tanner, DB
Tapai, M
Tarabrin, SP
Taracchini, A
Taylor, R
Theeg, T
Thirugnanasambandam, MP
Thomas, EG
Thomas, M
Thomas, P
Thorne, KA
Thorne, KS
Thrane, E
Tiwari, S
Tiwari, V
Tokmakov, KV
Tomlinson, C
Tonelli, M
Torres, CV
Torrie, CI
Toeyrae, D
Travasso, F
Traylor, G
Trifiro, D
Tringali, MC
Trozzo, L
Tse, M
Turconi, M
Tuyenbayev, D
Ugolini, D
Unnikrishnan, CS
Urban, AL
Usman, SA
Vahlbruch, H
Vajente, G
Valdes, G
van Bakel, N
van Beuzekom, M
van den Brand, JFJ
Van den Broeck, C
Vander-Hyde, DC
van der Schaaf, L
van Heijningen, JV
van Veggel, AA
Vardaro, M
Vass, S
Vasuth, M
Vaulin, R
Vecchio, A
Vedovato, G
Veitch, J
Veitch, PJ
Venkateswara, K
Verkindt, D
Vetrano, F
Vicere, A
Vinciguerra, S
Vine, DJ
Vinet, JY
Vitale, S
Vo, T
Vocca, H
Vorvick, C
Voss, D
Vousden, WD
Vyatchanin, SP
Wade, AR
Wade, LE
Wade, M
Walker, M
Wallace, L
Walsh, S
Wang, G
Wang, H
Wang, M
Wang, X
Wang, Y
Ward, RL
Warner, J
Was, M
Weaver, B
Wei, LW
Weinert, M
Weinstein, AJ
Weiss, R
Welborn, T
Wen, L
Wessels, P
Westphal, T
Wette, K
Whelan, JT
Whitcomb, SE
White, DJ
Whiting, BF
Williams, RD
Williamson, AR
Willis, JL
Willke, B
Wimmer, MH
Winkler, W
Wipf, CC
Wittel, H
Woan, G
Worden, J
Wright, JL
Wu, G
Yablon, J
Yam, W
Yamamoto, H
Yancey, CC
Yap, MJ
Yu, H
Yvert, M
Zadrozny, A
Zangrando, L
Zanolin, M
Zendri, JP
Zevin, M
Zhang, F
Zhang, L
Zhang, M
Zhang, Y
Zhao, C
Zhou, M
Zhou, Z
Zhu, XJ
Zucker, ME
Zuraw, SE
Zweizig, J
AF Abbott, B. P.
Abbott, R.
Abbott, T. D.
Abernathy, M. R.
Acernese, F.
Ackley, K.
Adams, C.
Adams, T.
Addesso, P.
Adhikari, R. X.
Adya, V. B.
Affeldt, C.
Agathos, M.
Agatsuma, K.
Aggarwal, N.
Aguiar, O. D.
Aiello, L.
Ain, A.
Ajith, P.
Allen, B.
Allocca, A.
Altin, P. A.
Anderson, S. B.
Anderson, W. G.
Arai, K.
Araya, M. C.
Arceneaux, C. C.
Areeda, J. S.
Arnaud, N.
Arun, K. G.
Ascenzi, S.
Ashton, G.
Ast, M.
Aston, S. M.
Astone, P.
Aufmuth, P.
Aulbert, C.
Babak, S.
Bacon, P.
Bader, M. K. M.
Baker, P. T.
Baldaccini, F.
Ballardin, G.
Ballmer, S. W.
Barayoga, J. C.
Barclay, S. E.
Barish, B. C.
Barker, D.
Barone, F.
Barr, B.
Barsotti, L.
Barsuglia, M.
Barta, D.
Bartlett, J.
Bartos, I.
Bassiri, R.
Basti, A.
Batch, J. C.
Baune, C.
Bavigadda, V.
Bazzan, M.
Behnke, B.
Bejger, M.
Bell, A. S.
Bell, C. J.
Berger, B. K.
Bergman, J.
Bergmann, G.
Berry, C. P. L.
Bersanetti, D.
Bertolini, A.
Betzwieser, J.
Bhagwat, S.
Bhandare, R.
Bilenko, I. A.
Billingsley, G.
Birch, J.
Birney, R.
Biscans, S.
Bisht, A.
Bitossi, M.
Biwer, C.
Bizouard, M. A.
Blackburn, J. K.
Blair, C. D.
Blair, D. G.
Blair, R. M.
Bloemen, S.
Bock, O.
Bodiya, T. P.
Boer, M.
Bogaert, G.
Bogan, C.
Bohe, A.
Bojtos, P.
Bond, C.
Bondu, F.
Bonnand, R.
Boom, B. A.
Bork, R.
Boschi, V.
Bose, S.
Bouffanais, Y.
Bozzi, A.
Bradaschia, C.
Brady, P. R.
Braginsky, V. B.
Branchesi, M.
Brau, J. E.
Briant, T.
Brillet, A.
Brinkmann, M.
Brisson, V.
Brockill, P.
Brooks, A. F.
Brown, D. A.
Brown, D. D.
Brown, N. M.
Buchanan, C. C.
Buikema, A.
Bulik, T.
Bulten, H. J.
Buonanno, A.
Buskulic, D.
Buy, C.
Byer, R. L.
Cadonati, L.
Cagnoli, G.
Cahillane, C.
Bustillo, J. Calderon
Callister, T.
Calloni, E.
Camp, J. B.
Cannon, K. C.
Cao, J.
Capano, C. D.
Capocasa, E.
Carbognani, F.
Caride, S.
Diaz, J. Casanueva
Casentini, C.
Caudill, S.
Cavaglia, M.
Cavalier, F.
Cavalieri, R.
Cella, G.
Cepeda, C. B.
Baiardi, L. Cerboni
Cerretani, G.
Cesarini, E.
Chakraborty, R.
Chalermsongsak, T.
Chamberlin, S. J.
Chan, M.
Chao, S.
Charlton, P.
Chassande-Mottin, E.
Chen, H. Y.
Chen, Y.
Cheng, C.
Chincarini, A.
Chiummo, A.
Cho, H. S.
Cho, M.
Chow, J. H.
Christensen, N.
Chu, Q.
Chua, S.
Chung, S.
Ciani, G.
Clara, F.
Clark, J. A.
Cleva, F.
Coccia, E.
Cohadon, P. -F.
Colla, A.
Collette, C. G.
Cominsky, L.
Constancio, M., Jr.
Conte, A.
Conti, L.
Cook, D.
Corbitt, T. R.
Cornish, N.
Corsi, A.
Cortese, S.
Costa, C. A.
Coughlin, M. W.
Coughlin, S. B.
Coulon, J. -P.
Countryman, S. T.
Couvares, P.
Cowan, E. E.
Coward, D. M.
Cowart, M. J.
Coyne, D. C.
Coyne, R.
Craig, K.
Creighton, J. D. E.
Cripe, J.
Crowder, S. G.
Cumming, A.
Cunningham, L.
Cuoco, E.
Dal Canton, T.
Danilishin, S. L.
D'Antonio, S.
Danzmann, K.
Darman, N. S.
Dattilo, V.
Dave, I.
Daveloza, H. P.
Davier, M.
Davies, G. S.
Daw, E. J.
Day, R.
DeBra, D.
Debreczeni, G.
Degallaix, J.
De Laurentis, M.
Deleglise, S.
Del Pozzo, W.
Denker, T.
Dent, T.
Dereli, H.
Dergachev, V.
DeRosa, R. T.
De Rosa, R.
DeSalvo, R.
Dhurandhar, S.
Diaz, M. C.
Di Fiore, L.
Di Giovanni, M.
Di Lieto, A.
Di Pace, S.
Di Palma, I.
Di Virgilio, A.
Dojcinoski, G.
Dolique, V.
Donovan, F.
Dooley, K. L.
Doravari, S.
Douglas, R.
Downes, T. P.
Drago, M.
Drever, R. W. P.
Driggers, J. C.
Du, Z.
Ducrot, M.
Dwyer, S. E.
Edo, T. B.
Edwards, M. C.
Effler, A.
Eggenstein, H. -B.
Ehrens, P.
Eichholz, J.
Eikenberry, S. S.
Engels, W.
Essick, R. C.
Etzel, T.
Evans, M.
Evans, T. M.
Everett, R.
Factourovich, M.
Fafone, V.
Fair, H.
Fairhurst, S.
Fan, X.
Fang, Q.
Farinon, S.
Farr, B.
Farr, W. M.
Favata, M.
Fays, M.
Fehrmann, H.
Fejer, M. M.
Ferrante, I.
Ferreira, E. C.
Ferrini, F.
Fidecaro, F.
Fiori, I.
Fiorucci, D.
Fisher, R. P.
Flaminio, R.
Fletcher, M.
Fournier, J. -D.
Franco, S.
Frasca, S.
Frasconi, F.
Frei, Z.
Freise, A.
Frey, R.
Frey, V.
Fricke, T. T.
Fritschel, P.
Frolov, V. V.
Fulda, P.
Fyffe, M.
Gabbard, H. A. G.
Gair, J. R.
Gammaitoni, L.
Gaonkar, S. G.
Garufi, F.
Gatto, A.
Gaur, G.
Gehrels, N.
Gemme, G.
Gendre, B.
Genin, E.
Gennai, A.
George, J.
Gergely, L.
Germain, V.
Ghosh, Archisman
Ghosh, S.
Giaime, J. A.
Giardina, K. D.
Giazotto, A.
Gill, K.
Glaefke, A.
Goetz, E.
Goetz, R.
Gondan, L.
Gonzalez, G.
Castro, J. M. Gonzalez
Gopakumar, A.
Gordon, N. A.
Gorodetsky, M. L.
Gossan, S. E.
Gosselin, M.
Gouaty, R.
Graef, C.
Graff, P. B.
Granata, M.
Grant, A.
Gras, S.
Gray, C.
Greco, G.
Green, A. C.
Groot, P.
Grote, H.
Grunewald, S.
Guidi, G. M.
Guo, X.
Gupta, A.
Gupta, M. K.
Gushwa, K. E.
Gustafson, E. K.
Gustafson, R.
Hacker, J. J.
Hall, B. R.
Hall, E. D.
Hammond, G.
Haney, M.
Hanke, M. M.
Hanks, J.
Hanna, C.
Hannam, M. D.
Hanson, J.
Hardwick, T.
Haris, K.
Harms, J.
Harry, G. M.
Harry, I. W.
Hart, M. J.
Hartman, M. T.
Haster, C. -J.
Haughian, K.
Heidmann, A.
Heintze, M. C.
Heitmann, H.
Hello, P.
Hemming, G.
Hendry, M.
Heng, I. S.
Hennig, J.
Heptonstall, A. W.
Heurs, M.
Hild, S.
Hoak, D.
Hodge, K. A.
Hofman, D.
Hollitt, S. E.
Holt, K.
Holz, D. E.
Hopkins, P.
Hosken, D. J.
Hough, J.
Houston, E. A.
Howell, E. J.
Hu, Y. M.
Huang, S.
Huerta, E. A.
Huet, D.
Hughey, B.
Husa, S.
Huttner, S. H.
Huynh-Dinh, T.
Idrisy, A.
Indik, N.
Ingram, D. R.
Inta, R.
Isa, H. N.
Isac, J. -M.
Isi, M.
Islas, G.
Isogai, T.
Iyer, B. R.
Izumi, K.
Jacqmin, T.
Jang, H.
Jani, K.
Jaranowski, P.
Jawahar, S.
Jimenez-Forteza, F.
Johnson, W. W.
Jones, D. I.
Jones, R.
Jonker, R. J. G.
Ju, L.
Kalaghatgi, C. V.
Kalogera, V.
Kandhasamy, S.
Kang, G.
Kanner, J. B.
Karki, S.
Kasprzack, M.
Katsavounidis, E.
Katzman, W.
Kaufer, S.
Kaur, T.
Kawabe, K.
Kawazoe, F.
Kefelian, F.
Kehl, M. S.
Keitel, D.
Kelley, D. B.
Kells, W.
Kennedy, R.
Key, J. S.
Khalaidovski, A.
Khalili, F. Y.
Khan, I.
Khan, S.
Khan, Z.
Khazanov, E. A.
Kijbunchoo, N.
Kim, C.
Kim, J.
Kim, K.
Kim, Nam-Gyu
Kim, Namjun
Kim, Y. -M.
King, E. J.
King, P. J.
Kinzel, D. L.
Kissel, J. S.
Kleybolte, L.
Klimenko, S.
Koehlenbeck, S. M.
Kokeyama, K.
Koley, S.
Kondrashov, V.
Kontos, A.
Korobko, M.
Korth, W. Z.
Kowalska, I.
Kozak, D. B.
Kringel, V.
Krolak, A.
Krueger, C.
Kuehn, G.
Kumar, P.
Kuo, L.
Kutynia, A.
Lackey, B. D.
Landry, M.
Lange, J.
Lantz, B.
Lasky, P. D.
Lazzarini, A.
Lazzaro, C.
Leaci, P.
Leavey, S.
Lebigot, E. O.
Lee, C. H.
Lee, H. K.
Lee, H. M.
Lee, K.
Lenon, A.
Leonardi, M.
Leong, J. R.
Leroy, N.
Letendre, N.
Levin, Y.
Levine, B. M.
Li, T. G. F.
Libson, A.
Littenberg, T. B.
Lockerbie, N. A.
Logue, J.
Lombardi, A. L.
Lord, J. E.
Lorenzini, M.
Loriette, V.
Lormand, M.
Losurdo, G.
Lough, J. D.
Lueck, H.
Lundgren, A. P.
Luo, J.
Lynch, R.
Ma, Y.
MacDonald, T.
Machenschalk, B.
MacInnis, M.
Macleod, D. M.
Magana-Sandoval, F.
Magee, R. M.
Mageswaran, M.
Majorana, E.
Maksimovic, I.
Malvezzi, V.
Man, N.
Mandel, I.
Mandic, V.
Mangano, V.
Mansell, G. L.
Manske, M.
Mantovani, M.
Marchesoni, F.
Marion, F.
Marka, S.
Marka, Z.
Markosyan, A. S.
Maros, E.
Martelli, F.
Martellini, L.
Martin, I. W.
Martin, R. M.
Martynov, D. V.
Marx, J. N.
Mason, K.
Masserot, A.
Massinger, T. J.
Masso-Reid, M.
Matichard, F.
Matone, L.
Mavalvala, N.
Mazumder, N.
Mazzolo, G.
McCarthy, R.
McClelland, D. E.
McCormick, S.
McGuire, S. C.
McIntyre, G.
McIver, J.
McManus, D. J.
McWilliams, S. T.
Meacher, D.
Meadors, G. D.
Meidam, J.
Melatos, A.
Mendell, G.
Mendoza-Gandara, D.
Mercer, R. A.
Merilh, E.
Merzougui, M.
Meshkov, S.
Messenger, C.
Messick, C.
Meyers, P. M.
Mezzani, F.
Miao, H.
Michel, C.
Middleton, H.
Mikhailov, E. E.
Milano, L.
Miller, J.
Millhouse, M.
Minenkov, Y.
Ming, J.
Mirshekari, S.
Mishra, C.
Mitra, S.
Mitrofanov, V. P.
Mitselmakher, G.
Mittleman, R.
Moggi, A.
Mohan, M.
Mohapatra, S. R. P.
Montani, M.
Moore, B. C.
Moore, C. J.
Moraru, D.
Moreno, G.
Morriss, S. R.
Mossavi, K.
Mours, B.
Mow-Lowry, C. M.
Mueller, C. L.
Mueller, G.
Muir, A. W.
Mukherjee, Arunava
Mukherjee, D.
Mukherjee, S.
Mukund, N.
Mullavey, A.
Munch, J.
Murphy, D. J.
Murray, P. G.
Mytidis, A.
Nardecchia, I.
Naticchioni, L.
Nayak, R. K.
Necula, V.
Nedkova, K.
Nelemans, G.
Neri, M.
Neunzert, A.
Newton, G.
Nguyen, T. T.
Nielsen, A. B.
Nissanke, S.
Nitz, A.
Nocera, F.
Nolting, D.
Normandin, M. E.
Nuttall, L. K.
Oberling, J.
Ochsner, E.
O'Dell, J.
Oelker, E.
Ogin, G. H.
Oh, J. J.
Oh, S. H.
Ohme, F.
Oliver, M.
Oppermann, P.
Oram, Richard J.
O'Reilly, B.
O'Shaughnessy, R.
Ottaway, D. J.
Ottens, R. S.
Overmier, H.
Owen, B. J.
Pai, A.
Pai, S. A.
Palamos, J. R.
Palashov, O.
Palomba, C.
Pal-Singh, A.
Pan, H.
Pankow, C.
Pannarale, F.
Pant, B. C.
Paoletti, F.
Paoli, A.
Papa, M. A.
Paris, H. R.
Parker, W.
Pascucci, D.
Pasqualetti, A.
Passaquieti, R.
Passuello, D.
Patricelli, B.
Patrick, Z.
Pearlstone, B. L.
Pedraza, M.
Pedurand, R.
Pekowsky, L.
Pele, A.
Penn, S.
Perreca, A.
Phelps, M.
Piccinni, O.
Pichot, M.
Piergiovanni, F.
Pierro, V.
Pillant, G.
Pinard, L.
Pinto, I. M.
Pitkin, M.
Poggiani, R.
Popolizio, P.
Post, A.
Powell, J.
Prasad, J.
Predoi, V.
Premachandra, S. S.
Prestegard, T.
Price, L. R.
Prijatelj, M.
Principe, M.
Privitera, S.
Prodi, G. A.
Prokhorov, L.
Puncken, O.
Punturo, M.
Puppo, P.
Puerrer, M.
Qi, H.
Qin, J.
Quetschke, V.
Quintero, E. A.
Quitzow-James, R.
Raab, F. J.
Rabeling, D. S.
Radkins, H.
Raffai, P.
Raja, S.
Rakhmanov, M.
Rapagnani, P.
Raymond, V.
Razzano, M.
Re, V.
Read, J.
Reed, C. M.
Regimbau, T.
Rei, L.
Reid, S.
Reitze, D. H.
Rew, H.
Reyes, S. D.
Ricci, F.
Riles, K.
Robertson, N. A.
Robie, R.
Robinet, F.
Rocchi, A.
Rolland, L.
Rollins, J. G.
Roma, V. J.
Romano, R.
Romanov, G.
Romie, J. H.
Rosinska, D.
Rowan, S.
Ruediger, A.
Ruggi, P.
Ryan, K.
Sachdev, S.
Sadecki, T.
Sadeghian, L.
Salconi, L.
Saleem, M.
Salemi, F.
Samajdar, A.
Sammut, L.
Sanchez, E. J.
Sandberg, V.
Sandeen, B.
Sanders, J. R.
Sassolas, B.
Sathyaprakash, B. S.
Saulson, P. R.
Sauter, O.
Savage, R. L.
Sawadsky, A.
Schale, P.
Schilling, R.
Schmidt, J.
Schmidt, P.
Schnabel, R.
Schofield, R. M. S.
Schoenbeck, A.
Schreiber, E.
Schuette, D.
Schutz, B. F.
Scott, J.
Scott, S. M.
Sellers, D.
Sengupta, A. S.
Sentenac, D.
Sequino, V.
Sergeev, A.
Serna, G.
Setyawati, Y.
Sevigny, A.
Shaddock, D. A.
Shah, S.
Shahriar, M. S.
Shaltev, M.
Shao, Z.
Shapiro, B.
Shawhan, P.
Sheperd, A.
Shoemaker, D. H.
Shoemaker, D. M.
Siellez, K.
Siemens, X.
Sigg, D.
Silva, A. D.
Simakov, D.
Singer, A.
Singer, L. P.
Singh, A.
Singh, R.
Singhal, A.
Sintes, A. M.
Slagmolen, B. J. J.
Smith, J. R.
Smith, N. D.
Smith, R. J. E.
Son, E. J.
Sorazu, B.
Sorrentino, F.
Souradeep, T.
Srivastava, A. K.
Staley, A.
Steinke, M.
Steinlechner, J.
Steinlechner, S.
Steinmeyer, D.
Stephens, B. C.
Stone, R.
Strain, K. A.
Straniero, N.
Stratta, G.
Strauss, N. A.
Strigin, S.
Sturani, R.
Stuver, A. L.
Summerscales, T. Z.
Sun, L.
Sutton, P. J.
Swinkels, B. L.
Szczepanczyk, M. J.
Tacca, M.
Talukder, D.
Tanner, D. B.
Tapai, M.
Tarabrin, S. P.
Taracchini, A.
Taylor, R.
Theeg, T.
Thirugnanasambandam, M. P.
Thomas, E. G.
Thomas, M.
Thomas, P.
Thorne, K. A.
Thorne, K. S.
Thrane, E.
Tiwari, S.
Tiwari, V.
Tokmakov, K. V.
Tomlinson, C.
Tonelli, M.
Torres, C. V.
Torrie, C. I.
Toeyrae, D.
Travasso, F.
Traylor, G.
Trifiro, D.
Tringali, M. C.
Trozzo, L.
Tse, M.
Turconi, M.
Tuyenbayev, D.
Ugolini, D.
Unnikrishnan, C. S.
Urban, A. L.
Usman, S. A.
Vahlbruch, H.
Vajente, G.
Valdes, G.
van Bakel, N.
van Beuzekom, M.
van den Brand, J. F. J.
Van den Broeck, C.
Vander-Hyde, D. C.
van der Schaaf, L.
van Heijningen, J. V.
van Veggel, A. A.
Vardaro, M.
Vass, S.
Vasuth, M.
Vaulin, R.
Vecchio, A.
Vedovato, G.
Veitch, J.
Veitch, P. J.
Venkateswara, K.
Verkindt, D.
Vetrano, F.
Vicere, A.
Vinciguerra, S.
Vine, D. J.
Vinet, J. -Y.
Vitale, S.
Vo, T.
Vocca, H.
Vorvick, C.
Voss, D.
Vousden, W. D.
Vyatchanin, S. P.
Wade, A. R.
Wade, L. E.
Wade, M.
Walker, M.
Wallace, L.
Walsh, S.
Wang, G.
Wang, H.
Wang, M.
Wang, X.
Wang, Y.
Ward, R. L.
Warner, J.
Was, M.
Weaver, B.
Wei, L. -W.
Weinert, M.
Weinstein, A. J.
Weiss, R.
Welborn, T.
Wen, L.
Wessels, P.
Westphal, T.
Wette, K.
Whelan, J. T.
Whitcomb, S. E.
White, D. J.
Whiting, B. F.
Williams, R. D.
Williamson, A. R.
Willis, J. L.
Willke, B.
Wimmer, M. H.
Winkler, W.
Wipf, C. C.
Wittel, H.
Woan, G.
Worden, J.
Wright, J. L.
Wu, G.
Yablon, J.
Yam, W.
Yamamoto, H.
Yancey, C. C.
Yap, M. J.
Yu, H.
Yvert, M.
Zadrozny, A.
Zangrando, L.
Zanolin, M.
Zendri, J. -P.
Zevin, M.
Zhang, F.
Zhang, L.
Zhang, M.
Zhang, Y.
Zhao, C.
Zhou, M.
Zhou, Z.
Zhu, X. J.
Zucker, M. E.
Zuraw, S. E.
Zweizig, J.
CA LIGO Sci Collaboration
Virgo Collaboration
TI GW150914: The Advanced LIGO Detectors in the Era of First Discoveries
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID GRAVITATIONAL-WAVE DETECTORS; THERMAL NOISE; INTERFEROMETERS; RADIATION
AB Following a major upgrade, the two advanced detectors of the Laser Interferometer Gravitational-wave Observatory (LIGO) held their first observation run between September 2015 and January 2016. With a strain sensitivity of 10(-23) / root Hz at 100 Hz, the product of observable volume and measurement time exceeded that of all previous runs within the first 16 days of coincident observation. On September 14, 2015, the Advanced LIGO detectors observed a transient gravitational-wave signal determined to be the coalescence of two black holes [B. P. Abbott et al., Phys. Rev. Lett. 116, 061102 (2016)], launching the era of gravitational-wave astronomy. The event, GW150914, was observed with a combined signal-to-noise ratio of 24 in coincidence by the two detectors. Here, we present the main features of the detectors that enabled this observation. At full sensitivity, the Advanced LIGO detectors are designed to deliver another factor of 3 improvement in the signal-to-noise ratio for binary black hole systems similar in mass to GW150914.
C1 [Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Anderson, S. B.; Arai, K.; Araya, M. C.; Barayoga, J. C.; Barish, B. C.; Berger, B. K.; Billingsley, G.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cahillane, C.; Callister, T.; Cepeda, C. B.; Chakraborty, R.; Chalermsongsak, T.; Couvares, P.; Coyne, D. C.; Dergachev, V.; Drever, R. W. P.; Ehrens, P.; Etzel, T.; Gossan, S. E.; Gushwa, K. E.; Gustafson, E. K.; Hall, E. D.; Heptonstall, A. W.; Hodge, K. A.; Isi, M.; Kanner, J. B.; Kells, W.; Kondrashov, V.; Korth, W. Z.; Kozak, D. B.; Lazzarini, A.; Li, T. G. F.; Mageswaran, M.; Maros, E.; Martynov, D. V.; Marx, J. N.; McIntyre, G.; McIver, J.; Meshkov, S.; Pedraza, M.; Perreca, A.; Price, L. R.; Quintero, E. A.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sachdev, S.; Sanchez, E. J.; Schmidt, P.; Shao, Z.; Singer, A.; Smith, N. D.; Smith, R. J. E.; Taylor, R.; Thirugnanasambandam, M. P.; Torrie, C. I.; Vajente, G.; Vass, S.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Williams, R. D.; Wipf, C. C.; Yamamoto, H.; Zhang, L.; Zucker, M. E.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Abbott, T. D.; Buchanan, C. C.; Corbitt, T. R.; Cripe, J.; Giaime, J. A.; Gonzalez, G.; Hardwick, T.; Johnson, W. W.; Kasprzack, M.; Kokeyama, K.; Macleod, D. M.; Singh, R.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Acernese, F.; Addesso, P.; Barone, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy.
[Acernese, F.; Barone, F.; Calloni, E.; De Laurentis, M.; De Rosa, R.; Di Fiore, L.; Garufi, F.; Milano, L.; Romano, R.] Ist Nazl Fis Nucl, Sez Napoli, Complesso Univ Monte St Angelo, I-80126 Naples, Italy.
[Ackley, K.; Ciani, G.; Eichholz, J.; Eikenberry, S. S.; Fulda, P.; Goetz, R.; Hartman, M. T.; Heintze, M. C.; Klimenko, S.; Martin, R. M.; Mitselmakher, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Necula, V.; Ottens, R. S.; Reitze, D. H.; Tanner, D. B.; Voss, D.; Whiting, B. F.] Univ Florida, Gainesville, FL 32611 USA.
[Adams, C.; Aston, S. M.; Betzwieser, J.; Birch, J.; Cowart, M. J.; DeRosa, R. T.; Doravari, S.; Effler, A.; Evans, T. M.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hanson, J.; Heintze, M. C.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Kinzel, D. L.; Lormand, M.; McCormick, S.; Mullavey, A.; Nolting, D.; Oram, Richard J.; O'Reilly, B.; Overmier, H.; Parker, W.; Pele, A.; Romie, J. H.; Sellers, D.; Stuver, A. L.; Thomas, M.; Thorne, K. A.; Traylor, G.; Welborn, T.; Wu, G.] LIGO Livingston Observ, Livingston, LA 70754 USA.
[Adams, T.; Bonnand, R.; Buskulic, D.; Ducrot, M.; Germain, V.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Verkindt, D.; Was, M.; Yvert, M.] Univ Savoie Mt Blanc, LAPP, CNRS IN2P3, F-74941 Annecy Le Vieux, France.
[Adya, V. B.; Affeldt, C.; Allen, B.; Aufmuth, P.; Aulbert, C.; Baune, C.; Bergmann, G.; Bisht, A.; Bock, O.; Bogan, C.; Brinkmann, M.; Capano, C. D.; Dal Canton, T.; Danzmann, K.; Denker, T.; Dent, T.; Di Palma, I.; Doravari, S.; Drago, M.; Eggenstein, H. -B.; Fehrmann, H.; Fricke, T. T.; Grote, H.; Hanke, M. M.; Heurs, M.; Indik, N.; Kawazoe, F.; Keitel, D.; Khalaidovski, A.; Koehlenbeck, S. M.; Kringel, V.; Kuehn, G.; Leong, J. R.; Lough, J. D.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Mazzolo, G.; Meadors, G. D.; Mendoza-Gandara, D.; Ming, J.; Mossavi, K.; Nielsen, A. B.; Nitz, A.; Oppermann, P.; Papa, M. A.; Post, A.; Puncken, O.; Ruediger, A.; Salemi, F.; Schilling, R.; Schmidt, J.; Schreiber, E.; Schuette, D.; Shaltev, M.; Simakov, D.; Singh, A.; Steinke, M.; Steinmeyer, D.; Tarabrin, S. P.; Theeg, T.; Walsh, S.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Whelan, J. T.; Willke, B.; Wimmer, M. H.; Winkler, W.; Wittel, H.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Agathos, M.; Agatsuma, K.; Bader, M. K. M.; Bertolini, A.; Boom, B. A.; Bulten, H. J.; Ghosh, S.; Jonker, R. J. G.; Koley, S.; Meidam, J.; Nelemans, G.; Nissanke, S.; Setyawati, Y.; Shah, S.; van Bakel, N.; van Beuzekom, M.; van den Brand, J. F. J.; Van den Broeck, C.; van der Schaaf, L.; van Heijningen, J. V.] Nikhef, Sci Pk, Amsterdam, Netherlands.
[Aggarwal, N.; Barsotti, L.; Biscans, S.; Bodiya, T. P.; Brown, N. M.; Buikema, A.; Donovan, F.; Essick, R. C.; Evans, M.; Fritschel, P.; Gras, S.; Isogai, T.; Katsavounidis, E.; Kontos, A.; Libson, A.; Lynch, R.; MacInnis, M.; Mason, K.; Matichard, F.; Mavalvala, N.; Miller, J.; Mittleman, R.; Mohapatra, S. R. P.; Oelker, E.; Shoemaker, D. H.; Tse, M.; Vaulin, R.; Vitale, S.; Weiss, R.; Yam, W.; Yu, H.; Zhang, F.; Zucker, M. E.] MIT, LIGO, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Aguiar, O. D.; Constancio, M., Jr.; Costa, C. A.; Ferreira, E. C.; Silva, A. D.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Paulo, Brazil.
[Aiello, L.; Coccia, E.; Fafone, V.; Khan, I.; Lorenzini, M.; Singhal, A.; Tiwari, S.; Wang, G.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy.
[Aiello, L.; Ascenzi, S.; Casentini, C.; Cesarini, E.; Coccia, E.; D'Antonio, S.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Minenkov, Y.; Nardecchia, I.; Rocchi, A.; Sequino, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Ain, A.; Bose, S.; Dhurandhar, S.; Gaonkar, S. G.; Gupta, A.; Mitra, S.; Mukund, N.; Prasad, J.; Souradeep, T.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Ajith, P.; Ghosh, Archisman; Iyer, B. R.; Mishra, C.; Mukherjee, Arunava] Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bangalore 560012, Karnataka, India.
[Allen, B.; Anderson, W. G.; Brady, P. R.; Brockill, P.; Caudill, S.; Creighton, J. D. E.; Downes, T. P.; Manske, M.; Mercer, R. A.; Mukherjee, D.; Ochsner, E.; Papa, M. A.; Qi, H.; Sadeghian, L.; Sheperd, A.; Siemens, X.; Stephens, B. C.; Urban, A. L.; Walsh, S.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Allen, B.; Bisht, A.; Danzmann, K.; Denker, T.; Heurs, M.; Kaufer, S.; Kawazoe, F.; Krueger, C.; Lough, J. D.; Lueck, H.; Sawadsky, A.; Schuette, D.; Steinmeyer, D.; Vahlbruch, H.; Willke, B.; Wimmer, M. H.; Wittel, H.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Allocca, A.; Basti, A.; Boschi, V.; Cerretani, G.; Di Lieto, A.; Ferrante, I.; Fidecaro, F.; Castro, J. M. Gonzalez; Passaquieti, R.; Patricelli, B.; Poggiani, R.; Razzano, M.; Tonelli, M.] Univ Pisa, I-56127 Pisa, Italy.
[Allocca, A.; Basti, A.; Boschi, V.; Bradaschia, C.; Cella, G.; Cerretani, G.; Di Lieto, A.; Di Virgilio, A.; Ferrante, I.; Fidecaro, F.; Frasconi, F.; Gennai, A.; Giazotto, A.; Castro, J. M. Gonzalez; Moggi, A.; Paoletti, F.; Passaquieti, R.; Passuello, D.; Patricelli, B.; Poggiani, R.; Razzano, M.; Tonelli, M.; Trozzo, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Altin, P. A.; Chow, J. H.; Mansell, G. L.; McClelland, D. E.; McManus, D. J.; Nguyen, T. T.; Rabeling, D. S.; Scott, S. M.; Shaddock, D. A.; Slagmolen, B. J. J.; Wade, A. R.; Ward, R. L.; Yap, M. J.] Australian Natl Univ, GPO Box 4, Canberra, ACT 0200, Australia.
[Arceneaux, C. C.; Cavaglia, M.; Dooley, K. L.; Gabbard, H. A. G.; Kandhasamy, S.; Trifiro, D.] Univ Mississippi, University, MS 38677 USA.
[Areeda, J. S.; Hacker, J. J.; Islas, G.; Read, J.; Serna, G.; Smith, J. R.; Vander-Hyde, D. C.] Calif State Univ Fullerton, Fullerton, CA 92831 USA.
[Arnaud, N.; Bizouard, M. A.; Brisson, V.; Diaz, J. Casanueva; Cavalier, F.; Davier, M.; Franco, S.; Frey, V.; Hello, P.; Huet, D.; Kasprzack, M.; Leroy, N.; Robinet, F.] Univ Paris Saclay, Univ Paris Sud, CNRS IN2P3, LAL, F-91400 Orsay, France.
[Arun, K. G.; Kalaghatgi, C. V.] Chennai Math Inst, Siruseri 603103, India.
[Ascenzi, S.; Casentini, C.; Cesarini, E.; Coccia, E.; Fafone, V.; Malvezzi, V.; Nardecchia, I.; Re, V.; Sequino, V.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Ashton, G.; Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Ast, M.; Kleybolte, L.; Korobko, M.; Pal-Singh, A.; Schnabel, R.; Schoenbeck, A.] Univ Hamburg, D-22761 Hamburg, Germany.
[Astone, P.; Colla, A.; Conte, A.; Di Giovanni, M.; Di Pace, S.; Frasca, S.; Leaci, P.; Majorana, E.; Mezzani, F.; Naticchioni, L.; Palomba, C.; Piccinni, O.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
[Babak, S.; Behnke, B.; Bohe, A.; Buonanno, A.; Di Palma, I.; Grunewald, S.; Harry, I. W.; Leaci, P.; Meadors, G. D.; Ming, J.; Papa, M. A.; Privitera, S.; Puerrer, M.; Raymond, V.; Schutz, B. F.; Singh, A.; Taracchini, A.; Walsh, S.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany.
[Bacon, P.; Barsuglia, M.; Bouffanais, Y.; Buy, C.; Capocasa, E.; Chassande-Mottin, E.; Fiorucci, D.; Gatto, A.; Lebigot, E. O.; Tacca, M.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, APC,Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France.
[Baker, P. T.; Cornish, N.; Millhouse, M.] Montana State Univ, Bozeman, MT 59717 USA.
[Baldaccini, F.; Gammaitoni, L.; Travasso, F.; Vocca, H.] Univ Perugia, I-06123 Perugia, Italy.
[Baldaccini, F.; Gammaitoni, L.; Marchesoni, F.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Ballardin, G.; Bavigadda, V.; Bitossi, M.; Bozzi, A.; Carbognani, F.; Cavalieri, R.; Chiummo, A.; Cortese, S.; Cuoco, E.; Dattilo, V.; Day, R.; Ferrini, F.; Fiori, I.; Genin, E.; Gosselin, M.; Hemming, G.; Kasprzack, M.; Mantovani, M.; Mohan, M.; Nocera, F.; Paoletti, F.; Paoli, A.; Pasqualetti, A.; Pillant, G.; Popolizio, P.; Prijatelj, M.; Ruggi, P.; Salconi, L.; Sentenac, D.; Swinkels, B. L.] EGO, I-56021 Pisa, Italy.
[Ballmer, S. W.; Bhagwat, S.; Biwer, C.; Brown, D. A.; Fair, H.; Fisher, R. P.; Kelley, D. B.; Lackey, B. D.; Lenon, A.; Lord, J. E.; Magana-Sandoval, F.; Massinger, T. J.; Nuttall, L. K.; Pekowsky, L.; Reyes, S. D.; Sanders, J. R.; Saulson, P. R.; Usman, S. A.; Vander-Hyde, D. C.; Vo, T.] Syracuse Univ, Syracuse, NY 13244 USA.
[Barclay, S. E.; Barr, B.; Bell, A. S.; Bell, C. J.; Chan, M.; Craig, K.; Cumming, A.; Cunningham, L.; Danilishin, S. L.; Davies, G. S.; Douglas, R.; Fletcher, M.; Glaefke, A.; Gordon, N. A.; Graef, C.; Grant, A.; Hammond, G.; Hart, M. J.; Haughian, K.; Hendry, M.; Heng, I. S.; Hennig, J.; Hild, S.; Hough, J.; Houston, E. A.; Hu, Y. M.; Huttner, S. H.; Isa, H. N.; Jones, R.; Leavey, S.; Lee, K.; Logue, J.; Mangano, V.; Martin, I. W.; Masso-Reid, M.; Messenger, C.; Murray, P. G.; Newton, G.; Pascucci, D.; Pearlstone, B. L.; Phelps, M.; Pitkin, M.; Powell, J.; Robertson, N. A.; Robie, R.; Rowan, S.; Scott, J.; Sorazu, B.; Steinlechner, J.; Steinlechner, S.; Strain, K. A.; van Veggel, A. A.; Woan, G.; Wright, J. L.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Barker, D.; Bartlett, J.; Batch, J. C.; Bergman, J.; Blair, R. M.; Clara, F.; Cook, D.; Driggers, J. C.; Dwyer, S. E.; Gray, C.; Hanks, J.; Ingram, D. R.; Izumi, K.; Kawabe, K.; Kijbunchoo, N.; King, P. J.; Kissel, J. S.; Landry, M.; Levine, B. M.; McCarthy, R.; Mendell, G.; Merilh, E.; Moraru, D.; Moreno, G.; Oberling, J.; Raab, F. J.; Radkins, H.; Reed, C. M.; Ryan, K.; Sadecki, T.; Sandberg, V.; Savage, R. L.; Sevigny, A.; Sigg, D.; Thomas, P.; Vorvick, C.; Warner, J.; Weaver, B.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA.
[Barta, D.; Debreczeni, G.; Vasuth, M.] RMKI, Wigner RCP, Konkoly Thege Miklos Ut 29-33, H-1121 Budapest, Hungary.
[Bartos, I.; Countryman, S. T.; Factourovich, M.; Marka, S.; Marka, Z.; Matone, L.; Murphy, D. J.; Staley, A.] Columbia Univ, New York, NY 10027 USA.
[Bassiri, R.; Byer, R. L.; DeBra, D.; Fejer, M. M.; Kim, Namjun; Lantz, B.; MacDonald, T.; Markosyan, A. S.; Paris, H. R.; Patrick, Z.; Shapiro, B.] Stanford Univ, Stanford, CA 94305 USA.
[Bazzan, M.; Vardaro, M.] Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy.
[Bazzan, M.; Conti, L.; Lazzaro, C.; Vardaro, M.; Vedovato, G.; Zangrando, L.; Zendri, J. -P.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Acernese, F.; Bejger, M.; Rosinska, D.] CAMK PAN, PL-00716 Warsaw, Poland.
[Berry, C. P. L.; Bond, C.; Brown, D. D.; Del Pozzo, W.; Farr, W. M.; Freise, A.; Green, A. C.; Haster, C. -J.; Mandel, I.; Miao, H.; Middleton, H.; Mow-Lowry, C. M.; Thomas, E. G.; Toeyrae, D.; Vecchio, A.; Veitch, J.; Vinciguerra, S.; Vousden, W. D.; Wang, H.; Wang, M.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Bersanetti, D.; Neri, M.] Univ Genoa, I-16146 Genoa, Italy.
[Bersanetti, D.; Chincarini, A.; Farinon, S.; Gemme, G.; Neri, M.; Rei, L.; Sorrentino, F.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy.
[Bhandare, R.; Dave, I.; George, J.; Pai, S. A.; Pant, B. C.; Raja, S.] RRCAT, Indore 452013, Madhya Pradesh, India.
[Bilenko, I. A.; Braginsky, V. B.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L.; Strigin, S.; Vyatchanin, S. P.] Moscow MV Lomonosov State Univ, Fac Phys, Moscow 119991, Russia.
[Birney, R.; Reid, S.; Vine, D. J.] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland.
[Blair, C. D.; Blair, D. G.; Chu, Q.; Chung, S.; Coward, D. M.; Fang, Q.; Howell, E. J.; Ju, L.; Kaur, T.; Ma, Y.; Qin, J.; Wang, Y.; Wen, L.; Zhao, C.; Zhu, X. J.] Univ Western Australia, Crawley, WA 6009, Australia.
[Bloemen, S.; Ghosh, S.; Groot, P.; Nelemans, G.; Nissanke, S.; Setyawati, Y.; Shah, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Boer, M.; Bogaert, G.; Brillet, A.; Cleva, F.; Coulon, J. -P.; Dereli, H.; Fournier, J. -D.; Gendre, B.; Heitmann, H.; Kefelian, F.; Man, N.; Martellini, L.; Merzougui, M.; Pichot, M.; Regimbau, T.; Siellez, K.; Turconi, M.; Vinet, J. -Y.; Wei, L. -W.] Univ Cote dAzur, Artemis, CNRS, Observ Cote dAzur,CS 34229, Nice 4, France.
[Bojtos, P.; Frei, Z.; Gondan, L.; Raffai, P.] MTA Eotvos Univ, Lendulet Astrophys Res Grp, H-1117 Budapest, Hungary.
[Bondu, F.] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France.
[Bose, S.; Hall, B. R.; Magee, R. M.; Mazumder, N.] Washington State Univ, Pullman, WA 99164 USA.
[Branchesi, M.; Baiardi, L. Cerboni; Greco, G.; Guidi, G. M.; Harms, J.; Martelli, F.; Montani, M.; Piergiovanni, F.; Stratta, G.; Vetrano, F.; Vicere, A.] Univ Urbino Carlo Bo, I-61029 Urbino, Italy.
[Branchesi, M.; Baiardi, L. Cerboni; Greco, G.; Guidi, G. M.; Harms, J.; Losurdo, G.; Martelli, F.; Montani, M.; Piergiovanni, F.; Stratta, G.; Vetrano, F.; Vicere, A.] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Florence, Italy.
[Brau, J. E.; Frey, R.; Karki, S.; Palamos, J. R.; Quitzow-James, R.; Roma, V. J.; Schale, P.; Schofield, R. M. S.; Talukder, D.] Univ Oregon, Eugene, OR 97403 USA.
[Cannon, K. C.; Kehl, M. S.; Kumar, P.] Univ Paris 06, Sorbonne Univ, ENS PSL Res Univ, Lab Kastler Brossel,CNRS,Coll France, F-75005 Paris, France.
[Bulik, T.; Kowalska, I.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
[Bulten, H. J.; van den Brand, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands.
[Buonanno, A.; Cho, M.; Graff, P. B.; Shawhan, P.; Yancey, C. C.] Univ Maryland, College Pk, MD 20742 USA.
[Cadonati, L.; Bustillo, J. Calderon; Clark, J. A.; Cowan, E. E.; Jani, K.; Lazzaro, C.; Shoemaker, D. M.; Siellez, K.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Cadonati, L.; Bustillo, J. Calderon; Clark, J. A.; Cowan, E. E.; Jani, K.; Lazzaro, C.; Shoemaker, D. M.; Siellez, K.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Cagnoli, G.] Univ Lyon 1, Inst Lumiere Mat, UMR CNRS 5306, F-69622 Villeurbanne, France.
[Cagnoli, G.; Degallaix, J.; Dolique, V.; Flaminio, R.; Granata, M.; Hofman, D.; Michel, C.; Pedurand, R.; Pinard, L.; Sassolas, B.; Straniero, N.] Univ Lyon, IN2P3 CNRS, LMA, F-69622 Villeurbanne, Lyon, France.
[Bustillo, J. Calderon; Husa, S.; Jimenez-Forteza, F.; Keitel, D.; Oliver, M.; Sintes, A. M.] Univ Illes Balears, IEEC IAC3, E-07122 Palma De Mallorca, Spain.
[Calloni, E.; De Laurentis, M.; De Rosa, R.; Garufi, F.; Milano, L.] Univ Naples Federico II, Complesso Univ Monte St Angelo, I-80126 Naples, Italy.
[Camp, J. B.; Gehrels, N.; Singer, L. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cannon, K. C.; Kehl, M. S.; Kumar, P.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Cao, J.; Du, Z.; Fan, X.; Guo, X.; Lebigot, E. O.; Wang, X.] Tsinghua Univ, Beijing 100084, Peoples R China.
[Caride, S.; Corsi, A.; Coyne, R.; Inta, R.; Owen, B. J.] Texas Tech Univ, Lubbock, TX 79409 USA.
[Chamberlin, S. J.; Everett, R.; Hanna, C.; Idrisy, A.; Meacher, D.; Messick, C.] Penn State Univ, University Pk, PA 16802 USA.
[Chao, S.; Cheng, C.; Huang, S.; Kuo, L.; Pan, H.] Natl Tsing Hua Univ, Hsinchu 30013, Taiwan.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Chen, H. Y.; Farr, B.; Holz, D. E.] Univ Chicago, Chicago, IL 60637 USA.
[Chen, Y.; Engels, W.; Schmidt, P.; Thorne, K. S.] Caltech CaRT, Pasadena, CA 91125 USA.
[Cho, H. S.; Jang, H.; Kang, G.; Kim, C.; Kim, Nam-Gyu] Korea Inst Sci & Technol Informat, Daejeon 305806, South Korea.
[Christensen, N.; Coughlin, M. W.; Edwards, M. C.; Luo, J.; Strauss, N. A.] Carleton Coll, Northfield, MN 55057 USA.
[Colla, A.; Conte, A.; Di Giovanni, M.; Di Pace, S.; Frasca, S.; Leaci, P.; Mezzani, F.; Naticchioni, L.; Piccinni, O.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, Piazzale Aldo Moro 5, I-00185 Rome, Italy.
[Collette, C. G.] Univ Brussels, B-1050 Brussels, Belgium.
[Cominsky, L.] Sonoma State Univ, Rohnert Pk, CA 94928 USA.
[Coughlin, S. B.; Crowder, S. G.; Huerta, E. A.; Kalogera, V.; Pankow, C.; Sandeen, B.; Shahriar, M. S.; Yablon, J.; Zevin, M.; Zhou, M.; Zhou, Z.] Northwestern Univ, Evanston, IL 60208 USA.
[Mandic, V.; Meyers, P. M.; Prestegard, T.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Darman, N. S.; Melatos, A.; Sammut, L.; Sun, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
[Daveloza, H. P.; Diaz, M. C.; Key, J. S.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E.; Quetschke, V.; Rakhmanov, M.; Stone, R.; Torres, C. V.; Tuyenbayev, D.; Valdes, G.] Univ Texas Rio Grande Valley, Brownsville, TX 78520 USA.
[Daw, E. J.; Edo, T. B.; Kennedy, R.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Ist Nazl Fis Nucl, Sez Napoli, I-80100 Naples, Italy.
[Dojcinoski, G.; Favata, M.; Moore, B. C.] Montclair State Univ, Montclair, NJ 07043 USA.
[Drago, M.; Leonardi, M.; Prodi, G. A.; Tringali, M. C.] Univ Trento, Dipartimento Fis, I-38123 Povo, Trento, Italy.
[Drago, M.; Leonardi, M.; Prodi, G. A.; Tringali, M. C.] Ist Nazl Fis Nucl, Trento Inst Fundamental Phys & Applicat, I-38123 Povo, Trento, Italy.
[Fairhurst, S.; Fays, M.; Hannam, M. D.; Hopkins, P.; Kalaghatgi, C. V.; Khan, S.; Muir, A. W.; Ohme, F.; Pannarale, F.; Predoi, V.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Tiwari, V.; Williamson, A. R.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Flaminio, R.] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Gair, J. R.] Univ Edinburgh, Sch Math, Edinburgh EH9 3FD, Midlothian, Scotland.
[Gaur, G.; Sengupta, A. S.] Indian Inst Technol, Gandhinagar Ahmedabad 382424, Gujarat, India.
[Gaur, G.; Gupta, M. K.; Khan, Z.; Srivastava, A. K.] Inst Plasma Res, Bhat 382428, Gandhinagar, India.
[Gergely, L.; Tapai, M.] Univ Szeged, Dom Ter 9, H-6720 Szeged, Hungary.
[Gill, K.; Hughey, B.; Szczepanczyk, M. J.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Goetz, E.; Gustafson, R.; Neunzert, A.; Riles, K.; Sanders, J. R.; Sauter, O.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Gopakumar, A.; Haney, M.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India.
[Harry, G. M.] Amer Univ, Washington, DC 20016 USA.
[Hoak, D.; Lombardi, A. L.; Nedkova, K.; Zuraw, S. E.] Univ Massachusetts, Amherst, MA 01003 USA.
[Hollitt, S. E.; Hosken, D. J.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Huerta, E. A.; McWilliams, S. T.] W Virginia Univ, Morgantown, WV 26506 USA.
[Jaranowski, P.] Univ Bial Ystok, PL-15424 Bialystok, Poland.
[Jawahar, S.; Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
[Haris, K.; Pai, A.; Saleem, M.] IISER TVM, CET Campus, Trivandrum 695016, Kerala, India.
[Khazanov, E. A.; Palashov, O.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Kim, J.; Kim, Y. -M.; Lee, C. H.] Pusan Natl Univ, Busan 609735, South Korea.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Krolak, A.; Kutynia, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Lange, J.; O'Shaughnessy, R.; Whelan, J. T.; Zhang, Y.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Lasky, P. D.; Levin, Y.; Premachandra, S. S.; Sammut, L.; Thrane, E.] Monash Univ, Clayton, Vic 3800, Australia.
[Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Littenberg, T. B.] Univ Alabama, Huntsville, AL 35899 USA.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy.
[McGuire, S. C.] Southern Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.] A&M Coll, Baton Rouge, LA 70813 USA.
[Mikhailov, E. E.; Rew, H.; Romanov, G.; Zhang, M.] Coll William & Mary, Williamsburg, VA 23187 USA.
[Mirshekari, S.; Sturani, R.] Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, Brazil.
[Moore, C. J.] Univ Cambridge, Cambridge CB2 1TN, England.
[Nayak, R. K.; Samajdar, A.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[O'Dell, J.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England.
[Ogin, G. H.] Whitman Coll, 345 Boyer Ave, Walla Walla, WA 99362 USA.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Daejeon 305390, South Korea.
[Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Rosinska, D.] Univ Zielona Gora, Janusz Gil Inst Astron, PL-65265 Zielona Gora, Poland.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Trozzo, L.] Univ Siena, I-53100 Siena, Italy.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Wade, L. E.; Wade, M.] Kenyon Coll, Gambier, OH 43022 USA.
[Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI Zhu, Xingjiang/E-1501-2016; Cesarini, Elisabetta/C-4507-2017;
Steinlechner, Sebastian/D-5781-2013; Chow, Jong/A-3183-2008; Frey,
Raymond/E-2830-2016; Prokhorov, Leonid/I-2953-2012; Ciani,
Giacomo/G-1036-2011; Di Virgilio, Angela Dora Vittoria/E-9078-2015;
Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Gammaitoni,
Luca/B-5375-2009; Ferrante, Isidoro/F-1017-2012; Chen,
Yanbei/A-2604-2013; Sorrentino, Fiodor/M-6662-2016; Garufi,
Fabio/K-3263-2015; Strigin, Sergey/I-8337-2012; McClelland,
David/E-6765-2010; Losurdo, Giovanni/K-1241-2014; Bondu,
Francois/A-2071-2012; Travasso, Flavio/J-9595-2016; Tiwari,
Shubhanshu/R-8546-2016; Bartos, Imre/A-2592-2017; Punturo,
Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Frasconi,
Franco/K-1068-2016; Vicere, Andrea/J-1742-2012; Sigg,
Daniel/I-4308-2015; Groot, Paul/K-4391-2016; Kumar, Prem/B-6691-2009;
Lazzaro, Claudia/L-2986-2016; Stratta, Maria Giuliana/L-3045-2016; De
Laurentis, Martina/L-3022-2016; Pinto, Innocenzo/L-3520-2016; Conti,
Livia/F-8565-2013; Vecchio, Alberto/F-8310-2015; Graef,
Christian/J-3167-2015; Branchesi, Marica/P-2296-2015; Leonardi,
Matteo/G-9694-2015; Strain, Kenneth/D-5236-2011; Marchesoni,
Fabio/A-1920-2008; prodi, giovanni/B-4398-2010; Costa,
Cesar/G-7588-2012; Gemme, Gianluca/C-7233-2008; Puppo,
Paola/J-4250-2012; Iyer, Bala R./E-2894-2012; Nelemans,
Gijs/D-3177-2012; Piccinni, Ornella Juliana/C-1319-2016; Rocchi,
Alessio/O-9499-2015; Danilishin, Stefan/K-7262-2012; Tacca,
Matteo/J-1599-2015
OI Naticchioni, Luca/0000-0003-2918-0730; Scott, Jamie/0000-0001-6701-6515;
Callister, Thomas/0000-0001-9892-177X; Sorazu,
Borja/0000-0002-6178-3198; Zweizig, John/0000-0002-1521-3397; Del Pozzo,
Walter/0000-0003-3978-2030; Gendre, Bruce/0000-0002-9077-2025; Granata,
Massimo/0000-0003-3275-1186; Berry, Christopher/0000-0003-3870-7215;
O'Shaughnessy, Richard/0000-0001-5832-8517; Zhu,
Xingjiang/0000-0001-7049-6468; Boschi, Valerio/0000-0001-8665-2293;
Papa, M.Alessandra/0000-0002-1007-5298; Vocca,
Helios/0000-0002-1200-3917; Farr, Ben/0000-0002-2916-9200; Guidi,
Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431;
Collette, Christophe/0000-0002-4430-3703; Addesso,
Paolo/0000-0003-0895-184X; Kanner, Jonah/0000-0001-8115-0577; Mandel,
Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669;
Murphy, David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X;
Veitch, John/0000-0002-6508-0713; Davies, Gareth/0000-0002-4289-3439;
Principe, Maria/0000-0002-6327-0628; Cesarini,
Elisabetta/0000-0001-9127-3167; Steinlechner,
Sebastian/0000-0003-4710-8548; Chow, Jong/0000-0002-2414-5402; Frey,
Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di
Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Khan,
Sebastian/0000-0003-4953-5754; Dolique, Vincent/0000-0001-5644-9905;
Gammaitoni, Luca/0000-0002-4972-7062; Ferrante,
Isidoro/0000-0002-0083-7228; Sorrentino, Fiodor/0000-0002-9605-9829;
Garufi, Fabio/0000-0003-1391-6168; McClelland,
David/0000-0001-6210-5842; Losurdo, Giovanni/0000-0003-0452-746X; Bondu,
Francois/0000-0001-6487-5197; Travasso, Flavio/0000-0002-4653-6156;
Tiwari, Shubhanshu/0000-0003-1611-6625; Punturo,
Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338;
Frasconi, Franco/0000-0003-4204-6587; Vicere,
Andrea/0000-0003-0624-6231; Sigg, Daniel/0000-0003-4606-6526; Groot,
Paul/0000-0002-4488-726X; Lazzaro, Claudia/0000-0001-5993-3372; Stratta,
Maria Giuliana/0000-0003-1055-7980; De Laurentis,
Martina/0000-0002-3815-4078; Conti, Livia/0000-0003-2731-2656; Vecchio,
Alberto/0000-0002-6254-1617; Graef, Christian/0000-0002-4535-2603;
Strain, Kenneth/0000-0002-2066-5355; Marchesoni,
Fabio/0000-0001-9240-6793; prodi, giovanni/0000-0001-5256-915X; Gemme,
Gianluca/0000-0002-1127-7406; Puppo, Paola/0000-0003-4677-5015; Iyer,
Bala R./0000-0002-4141-5179; Nelemans, Gijs/0000-0002-0752-2974;
Piccinni, Ornella Juliana/0000-0001-5478-3950; Rocchi,
Alessio/0000-0002-1382-9016; Danilishin, Stefan/0000-0001-7758-7493;
Tacca, Matteo/0000-0003-1353-0441
FU Australian Research Council; EGO consortium; Council of Scientific and
Industrial Research of India; Department of Science and Technology,
India; Science AMP; Engineering Research Board (SERB), India; Ministry
of Human Resource Development, India; Spanish Ministerio de Economia y
Competitividad; Conselleria d'Economia i Competitivitat; Conselleria
d'Educacio, Cultura i Universitats of the Govern de les Illes Balears;
National Science Centre of Poland; European Commission; Royal Society;
Scottish Funding Council; Scottish Universities Physics Alliance;
Hungarian Scientific Research Fund (OTKA); Lyon Institute of Origins
(LIO); National Research Foundation of Korea; Industry Canada; Province
of Ontario through the Ministry of Economic Development and Innovation;
Natural Science and Engineering Research Council Canada; Canadian
Institute for Advanced Research; Brazilian Ministry of Science,
Technology, and Innovation; Russian Foundation for Basic Research;
Leverhulme Trust; Research Corporation, Ministry of Science and
Technology (MOST), Taiwan; Kavli Foundation
FX The authors gratefully acknowledge the support of the United States
National Science Foundation (NSF) for the construction and operation of
the LIGO Laboratory and Advanced LIGO as well as the Science and
Technology Facilities Council (STFC) of the United Kingdom, the
Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for
support of the construction of Advanced LIGO and construction and
operation of the GEO600 detector. Additional support for Advanced LIGO
was provided by the Australian Research Council. The authors gratefully
acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN),
the French Centre National de la Recherche Scientifique (CNRS) and the
Foundation for Fundamental Research on Matter supported by the
Netherlands Organisation for Scientific Research, for the construction
and operation of the Virgo detector and the creation and support of the
EGO consortium. The authors also gratefully acknowledge research support
from these agencies as well as by the Council of Scientific and
Industrial Research of India, Department of Science and Technology,
India, Science & Engineering Research Board (SERB), India, Ministry of
Human Resource Development, India, the Spanish Ministerio de Economia y
Competitividad, the Conselleria d'Economia i Competitivitat and
Conselleria d'Educacio, Cultura i Universitats of the Govern de les
Illes Balears, the National Science Centre of Poland, the European
Commission, the Royal Society, the Scottish Funding Council, the
Scottish Universities Physics Alliance, the Hungarian Scientific
Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National
Research Foundation of Korea, Industry Canada and the Province of
Ontario through the Ministry of Economic Development and Innovation, the
Natural Science and Engineering Research Council Canada, Canadian
Institute for Advanced Research, the Brazilian Ministry of Science,
Technology, and Innovation, Russian Foundation for Basic Research, the
Leverhulme Trust, the Research Corporation, Ministry of Science and
Technology (MOST), Taiwan and the Kavli Foundation. The authors
gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and
the State of Niedersachsen/Germany for provision of computational
resources. This document has been assigned the LIGO Laboratory Document
No. LIGO-P1500237.
NR 65
TC 47
Z9 47
U1 20
U2 61
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD MAR 31
PY 2016
VL 116
IS 13
AR 131103
DI 10.1103/PhysRevLett.116.131103
PG 12
WC Physics, Multidisciplinary
SC Physics
GA DH9EQ
UT WOS:000373099600002
ER
PT J
AU Abbott, BP
Abbott, R
Abbott, TD
Abernathy, MR
Acernese, F
Ackley, K
Adams, C
Adams, T
Addesso, P
Adhikari, RX
Adya, VB
Affeldt, C
Agathos, M
Agatsuma, K
Aggarwal, N
Aguiar, OD
Aiello, L
Ain, A
Ajith, P
Allen, B
Allocca, A
Altin, PA
Anderson, SB
Anderson, WG
Arai, K
Araya, MC
Arceneaux, CC
Areeda, JS
Arnaud, N
Arun, KG
Ascenzi, S
Ashton, G
Ast, M
Aston, SM
Astone, P
Aufmuth, P
Aulbert, C
Babak, S
Bacon, P
Bader, MKM
Baker, PT
Baldaccini, F
Ballardin, G
Ballmer, SW
Barayoga, JC
Barclay, SE
Barish, BC
Barker, D
Barone, F
Barr, B
Barsotti, L
Barsuglia, M
Barta, D
Bartlett, J
Bartos, I
Bassiri, R
Basti, A
Batch, JC
Baune, C
Bavigadda, V
Bazzan, M
Behnke, B
Bejger, M
Bell, AS
Bell, CJ
Berger, BK
Bergman, J
Bergmann, G
Berry, CPL
Bersanetti, D
Bertolini, A
Betzwieser, J
Bhagwat, S
Bhandare, R
Bilenko, IA
Billingsley, G
Birch, J
Birney, R
Biscans, S
Bisht, A
Bitossi, M
Biwer, C
Bizouard, MA
Blackburn, JK
Blair, CD
Blair, DG
Blair, M
Bloemen, S
Bock, O
Bodiya, TP
Boer, M
Bogaert, G
Bogan, C
Bohe, A
Bojtos, P
Bond, C
Bondu, F
Bonnand, R
Boom, BA
Bork, R
Boschi, V
Bose, S
Bouffanais, Y
Bozzi, A
Bradaschia, C
Brady, PR
Braginsky, VB
Branchesi, M
Brau, JE
Briant, T
Brillet, A
Brinkmann, M
Brisson, V
Brockill, P
Brooks, AF
Brown, DD
Brown, NM
Buchanan, CC
Buikema, A
Bulik, T
Bulten, HJ
Buonanno, A
Buskulic, D
Buy, C
Byer, RL
Cadonati, L
Cagnoli, G
Cahillane, C
Bustillo, JC
Callister, T
Calloni, E
Camp, JB
Cannon, KC
Cao, J
Capano, CD
Capocasa, E
Carbognani, F
Caride, S
Diaz, JC
Casentini, C
Caudill, S
Cavaglia, M
Cavalier, F
Cavalieri, R
Cella, G
Cepeda, CB
Baiardi, LC
Cerretani, G
Cesarini, E
Chakraborty, R
Chalermsongsak, T
Chamberlin, SJ
Chan, M
Chao, S
Charlton, P
Chassande-Mottin, E
Chen, HY
Chen, Y
Cheng, C
Chincarini, A
Chiummo, A
Cho, HS
Cho, M
Chow, JH
Christensen, N
Chu, Q
Chua, S
Chung, S
Ciani, G
Clara, F
Clark, JA
Cleva, F
Coccia, E
Cohadon, PF
Colla, A
Collette, CG
Cominsky, L
Constancio, M
Conte, A
Conti, L
Cook, D
Corbitt, TR
Cornish, N
Corsi, A
Cortese, S
Costa, CA
Coughlin, MW
Coughlin, SB
Coulon, JP
Countryman, ST
Couvares, P
Cowan, EE
Coward, DM
Cowart, MJ
Coyne, DC
Coyne, R
Craig, K
Creighton, JDE
Cripe, J
Crowder, SG
Cumming, A
Cunningham, L
Cuoco, E
Dal Canton, T
Danilishin, SL
D'Antonio, S
Danzmann, K
Darman, NS
Dattilo, V
Dave, I
Daveloza, HP
Davier, M
Davies, GS
Daw, EJ
Day, R
DeBra, D
Debreczeni, G
Degallaix, J
De Laurentis, M
Deleglise, S
Del Pozzo, W
Denker, T
Dent, T
Dereli, H
Dergachev, V
DeRosa, RT
De Rosa, R
DeSalvo, R
Dhurandhar, S
Diaz, MC
Di Fiore, L
Di Giovanni, M
Di Lieto, A
Di Pace, S
Di Palma, I
Di Virgilio, A
Dojcinoski, G
Dolique, V
Donovan, F
Dooley, KL
Doravari, S
Douglas, R
Downes, TP
Drago, M
Drever, RWP
Driggers, JC
Du, Z
Ducrot, M
Dwyer, SE
Edo, TB
Edwards, MC
Effler, A
Eggenstein, HB
Ehrens, P
Eichholz, J
Eikenberry, SS
Engels, W
Essick, RC
Etzel, T
Evans, M
Evans, TM
Everett, R
Factourovich, M
Fafone, V
Fair, H
Fairhurst, S
Fan, X
Fang, Q
Farinon, S
Farr, B
Farr, WM
Favata, M
Fays, M
Fehrmann, H
Fejer, MM
Ferrante, I
Ferreira, EC
Ferrini, F
Fidecaro, F
Fiori, I
Fiorucci, D
Fisher, RP
Flaminio, R
Fletcher, M
Fournier, JD
Franco, S
Frasca, S
Frasconi, F
Frei, Z
Freise, A
Frey, R
Frey, V
Fricke, TT
Fritschel, P
Frolov, VV
Fulda, P
Fyffe, M
Gabbard, HAG
Gair, JR
Gammaitoni, L
Gaonkar, SG
Garufi, F
Gatto, A
Gaur, G
Gehrels, N
Gemme, G
Gendre, B
Genin, E
Gennai, A
George, J
Gergely, L
Germain, V
Ghosh, A
Ghosh, S
Giaime, JA
Giardina, KD
Giazotto, A
Gill, K
Glaefke, A
Goetz, E
Goetz, R
Gondan, L
Gonzalez, G
Castro, JMG
Gopakumar, A
Gordon, NA
Gorodetsky, ML
Gossan, SE
Gosselin, M
Gouaty, R
Graef, C
Graff, PB
Granata, M
Grant, A
Gras, S
Gray, C
Greco, G
Green, AC
Groot, P
Grote, H
Grunewald, S
Guidi, GM
Guo, X
Gupta, A
Gupta, MK
Gushwa, KE
Gustafson, EK
Gustafson, R
Hacker, JJ
Hall, BR
Hall, ED
Hammond, G
Haney, M
Hanke, MM
Hanks, J
Hanna, C
Hannam, MD
Hanson, J
Hardwick, T
Haris, K
Harms, J
Harry, GM
Harry, IW
Hart, MJ
Hartman, MT
Haster, CJ
Haughian, K
Heidmann, A
Heintze, MC
Heitmann, H
Hello, P
Hemming, G
Hendry, M
Heng, IS
Hennig, J
Heptonstall, AW
Heurs, M
Hild, S
Hoak, D
Hodge, KA
Hofman, D
Hollitt, SE
Holt, K
Holz, DE
Hopkins, P
Hosken, DJ
Hough, J
Houston, EA
Howell, EJ
Hu, YM
Huang, S
Huerta, EA
Huet, D
Hughey, B
Husa, S
Huttner, SH
Huynh-Dinh, T
Idrisy, A
Indik, N
Ingram, DR
Inta, R
Isa, HN
Isac, JM
Isi, M
Islas, G
Isogai, T
Iyer, BR
Izumi, K
Jacqmin, T
Jang, H
Jani, K
Jaranowski, P
Jawahar, S
Jimenez-Forteza, F
Johnson, WW
Jones, DI
Jones, R
Jonker, RJG
Ju, L
Kalaghatgi, CV
Kalogera, V
Kandhasamy, S
Kang, G
Kanner, JB
Karki, S
Kasprzack, M
Katsavounidis, E
Katzman, W
Kaufer, S
Kaur, T
Kawabe, K
Kawazoe, F
Kefelian, F
Kehl, MS
Keitel, D
Kelley, DB
Kells, W
Kennedy, R
Key, JS
Khalaidovski, A
Khalili, FY
Khan, I
Khan, S
Khan, Z
Khazanov, EA
Kijbunchoo, N
Kim, C
Kim, J
Kim, K
Kim, NG
Kim, N
Kim, YM
King, EJ
King, PJ
Kinzel, DL
Kissel, JS
Kleybolte, L
Klimenko, S
Koehlenbeck, SM
Kokeyama, K
Koley, S
Kondrashov, V
Kontos, A
Korobko, M
Korth, WZ
Kowalska, I
Kozak, DB
Kringel, V
Krolak, A
Krueger, C
Kuehn, G
Kumar, P
Kuo, L
Kutynia, A
Lackey, BD
Landry, M
Lange, J
Lantz, B
Lasky, PD
Lazzarini, A
Lazzaro, C
Leaci, P
Leavey, S
Lebigot, EO
Lee, CH
Lee, HK
Lee, HM
Lee, K
Lenon, A
Leonardi, M
Leong, JR
Leroy, N
Letendre, N
Levin, Y
Levine, BM
Li, TGF
Libson, A
Littenberg, TB
Lockerbie, NA
Logue, J
Lombardi, AL
Lord, JE
Lorenzini, M
Loriette, V
Lormand, M
Losurdo, G
Lough, JD
Lueck, H
Lundgren, AP
Luo, J
Lynch, R
Ma, Y
MacDonald, T
Machenschalk, B
MacInnis, M
Macleod, DM
Magana-Sandoval, F
Magee, RM
Mageswaran, M
Majorana, E
Maksimovic, I
Malvezzi, V
Man, N
Mandel, I
Mandic, V
Mangano, V
Mansell, GL
Manske, M
Mantovani, M
Marchesoni, F
Marion, F
Marka, S
Marka, Z
Markosyan, AS
Maros, E
Martelli, F
Martellini, L
Martin, IW
Martin, RM
Martynov, DV
Marx, JN
Mason, K
Masserot, A
Massinger, TJ
Masso-Reid, M
Matichard, F
Matone, L
Mavalvala, N
Mazumder, N
Mazzolo, G
McCarthy, R
McClelland, DE
McCormick, S
McGuire, SC
McIntyre, G
McIver, J
McManus, DJ
McWilliams, ST
Meacher, D
Meadors, GD
Meidam, J
Melatos, A
Mendell, G
Mendoza-Gandara, D
Mercer, RA
Merilh, E
Merzougui, M
Meshkov, S
Messenger, C
Messick, C
Meyers, PM
Mezzani, F
Miao, H
Michel, C
Middleton, H
Mikhailov, EE
Milano, L
Miller, J
Millhouse, M
Minenkov, Y
Ming, J
Mirshekari, S
Mishra, C
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Moggi, A
Mohan, M
Mohapatra, SRP
Montani, M
Moore, BC
Moore, CJ
Moraru, D
Moreno, G
Morriss, SR
Mossavi, K
Mours, B
Mow-Lowry, CM
Mueller, CL
Mueller, G
Muir, AW
Mukherjee, A
Mukherjee, D
Mukherjee, S
Mukund, N
Mullavey, A
Munch, J
Murphy, DJ
Murray, PG
Mytidis, A
Nardecchia, I
Naticchioni, L
Nayak, RK
Necula, V
Nedkova, K
Nelemans, G
Neri, M
Neunzert, A
Newton, G
Nguyen, TT
Nielsen, AB
Nissanke, S
Nitz, A
Nocera, F
Nolting, D
Normandin, MEN
Nuttall, LK
Oberling, J
Ochsner, E
O'Dell, J
Oelker, E
Ogin, GH
Oh, JJ
Oh, SH
Ohme, F
Oliver, M
Oppermann, P
Oram, RJ
O'Reilly, B
O'Shaughnessy, R
Ottaway, DJ
Ottens, RS
Overmier, H
Owen, BJ
Pai, A
Pai, SA
Palamos, JR
Palashov, O
Palomba, C
Pal-Singh, A
Pan, H
Pankow, C
Pannarale, F
Pant, BC
Paoletti, F
Paoli, A
Papa, MA
Paris, HR
Parker, W
Pascucci, D
Pasqualetti, A
Passaquieti, R
Passuello, D
Patricelli, B
Patrick, Z
Pearlstone, BL
Pedraza, M
Pedurand, R
Pekowsky, L
Pele, A
Penn, S
Perreca, A
Phelps, M
Piccinni, O
Pichot, M
Piergiovanni, F
Pierro, V
Pillant, G
Pinard, L
Pinto, IM
Pitkin, M
Poggiani, R
Popolizio, P
Post, A
Powell, J
Prasad, J
Predoi, V
Premachandra, SS
Prestegard, T
Price, LR
Prijatelj, M
Principe, M
Privitera, S
Prodi, GA
Prokhorov, L
Puncken, O
Punturo, M
Puppo, P
Puerrer, M
Qi, H
Qin, J
Quetschke, V
Quintero, EA
Quitzow-James, R
Raab, FJ
Rabeling, DS
Radkins, H
Raffai, P
Raja, S
Rakhmanov, M
Rapagnani, P
Raymond, V
Razzano, M
Re, V
Read, J
Reed, CM
Regimbau, T
Rei, L
Reid, S
Reitze, DH
Rew, H
Reyes, SD
Ricci, F
Riles, K
Robertson, NA
Robie, R
Robinet, F
Rocchi, A
Rolland, L
Rollins, JG
Roma, VJ
Romano, JD
Romano, R
Romanov, G
Romie, JH
Rosinska, D
Rowan, S
Ruediger, A
Ruggi, P
Ryan, K
Sachdev, S
Sadecki, T
Sadeghian, L
Salconi, L
Saleem, M
Salemi, F
Samajdar, A
Sammut, L
Sanchez, EJ
Sandberg, V
Sandeen, B
Sanders, JR
Sassolas, B
Sathyaprakash, BS
Saulson, PR
Sauter, O
Savage, RL
Sawadsky, A
Schale, P
Schilling, R
Schmidt, J
Schmidt, P
Schnabel, R
Schofield, RMS
Schoenbeck, A
Schreiber, E
Schuette, D
Schutz, BF
Scott, J
Scott, SM
Sellers, D
Sentenac, D
Sequino, V
Sergeev, A
Serna, G
Setyawati, Y
Sevigny, A
Shaddock, DA
Shah, S
Shahriar, MS
Shaltev, M
Shao, Z
Shapiro, B
Shawhan, P
Sheperd, A
Shoemaker, DH
Shoemaker, DM
Siellez, K
Siemens, X
Sigg, D
Silva, AD
Simakov, D
Singer, A
Singer, LP
Singh, A
Singh, R
Singhal, A
Sintes, AM
Slagmolen, BJJ
Smith, JR
Smith, ND
Smith, RJE
Son, EJ
Sorazu, B
Sorrentino, F
Souradeep, T
Srivastava, AK
Staley, A
Steinke, M
Steinlechner, J
Steinlechner, S
Steinmeyer, D
Stephens, BC
Stone, R
Strain, KA
Straniero, N
Stratta, G
Strauss, NA
Strigin, S
Sturani, R
Stuver, AL
Summerscales, TZ
Sun, L
Sutton, PJ
Swinkels, BL
Szczepanczyk, MJ
Tacca, M
Talukder, D
Tanner, DB
Tapai, M
Tarabrin, SP
Taracchini, A
Taylor, R
Theeg, T
Thirugnanasambandam, MP
Thomas, EG
Thomas, M
Thomas, P
Thorne, KA
Thorne, KS
Thrane, E
Tiwari, S
Tiwari, V
Tokmakov, KV
Tomlinson, C
Tonelli, M
Torres, CV
Torrie, CI
Toeyrae, D
Travasso, F
Traylor, G
Trifiro, D
Tringali, MC
Trozzo, L
Tse, M
Turconi, M
Tuyenbayev, D
Ugolini, D
Unnikrishnan, CS
Urban, AL
Usman, SA
Vahlbruch, H
Vajente, G
Valdes, G
Van Bakel, N
Van Beuzekom, M
Van den Brand, JFJ
Van den Broeck, C
Vander-Hyde, DC
Van der Schaaf, L
van Heijningen, JV
van Veggel, AA
Vardaro, M
Vass, S
Vasuth, M
Vaulin, R
Vecchio, A
Vedovato, G
Veitch, J
Veitch, PJ
Venkateswara, K
Verkindt, D
Vetrano, F
Vicere, A
Vinciguerra, S
Vine, DJ
Vinet, JY
Vitale, S
Vo, T
Vocca, H
Vorvick, C
Voss, D
Vousden, WD
Vyatchanin, SP
Wade, AR
Wade, LE
Wade, M
Walker, M
Wallace, L
Walsh, S
Wang, G
Wang, H
Wang, M
Wang, X
Wang, Y
Ward, RL
Warner, J
Was, M
Weaver, B
Wei, LW
Weinert, M
Weinstein, AJ
Weiss, R
Welborn, T
Wen, L
Wessels, P
Westphal, T
Wette, K
Whelan, JT
White, DJ
Whiting, BF
Williams, RD
Williamson, AR
Willis, JL
Willke, B
Wimmer, MH
Winkler, W
Wipf, CC
Wittel, H
Woan, G
Worden, J
Wright, JL
Wu, G
Yablon, J
Yam, W
Yamamoto, H
Yancey, CC
Yap, MJ
Yu, H
Yvert, M
Zadrozny, A
Zangrando, L
Zanolin, M
Zendri, JP
Zevin, M
Zhang, F
Zhang, L
Zhang, M
Zhang, Y
Zhao, C
Zhou, M
Zhou, Z
Zhu, XJ
Zucker, ME
Zuraw, SE
Zweizig, J
AF Abbott, B. P.
Abbott, R.
Abbott, T. D.
Abernathy, M. R.
Acernese, F.
Ackley, K.
Adams, C.
Adams, T.
Addesso, P.
Adhikari, R. X.
Adya, V. B.
Affeldt, C.
Agathos, M.
Agatsuma, K.
Aggarwal, N.
Aguiar, O. D.
Aiello, L.
Ain, A.
Ajith, P.
Allen, B.
Allocca, A.
Altin, P. A.
Anderson, S. B.
Anderson, W. G.
Arai, K.
Araya, M. C.
Arceneaux, C. C.
Areeda, J. S.
Arnaud, N.
Arun, K. G.
Ascenzi, S.
Ashton, G.
Ast, M.
Aston, S. M.
Astone, P.
Aufmuth, P.
Aulbert, C.
Babak, S.
Bacon, P.
Bader, M. K. M.
Baker, P. T.
Baldaccini, F.
Ballardin, G.
Ballmer, S. W.
Barayoga, J. C.
Barclay, S. E.
Barish, B. C.
Barker, D.
Barone, F.
Barr, B.
Barsotti, L.
Barsuglia, M.
Barta, D.
Bartlett, J.
Bartos, I.
Bassiri, R.
Basti, A.
Batch, J. C.
Baune, C.
Bavigadda, V.
Bazzan, M.
Behnke, B.
Bejger, M.
Bell, A. S.
Bell, C. J.
Berger, B. K.
Bergman, J.
Bergmann, G.
Berry, C. P. L.
Bersanetti, D.
Bertolini, A.
Betzwieser, J.
Bhagwat, S.
Bhandare, R.
Bilenko, I. A.
Billingsley, G.
Birch, J.
Birney, R.
Biscans, S.
Bisht, A.
Bitossi, M.
Biwer, C.
Bizouard, M. A.
Blackburn, J. K.
Blair, C. D.
Blair, D. G.
Blair, M.
Bloemen, S.
Bock, O.
Bodiya, T. P.
Boer, M.
Bogaert, G.
Bogan, C.
Bohe, A.
Bojtos, P.
Bond, C.
Bondu, F.
Bonnand, R.
Boom, B. A.
Bork, R.
Boschi, V.
Bose, S.
Bouffanais, Y.
Bozzi, A.
Bradaschia, C.
Brady, P. R.
Braginsky, V. B.
Branchesi, M.
Brau, J. E.
Briant, T.
Brillet, A.
Brinkmann, M.
Brisson, V.
Brockill, P.
Brooks, A. F.
Brown, D. D.
Brown, N. M.
Buchanan, C. C.
Buikema, A.
Bulik, T.
Bulten, H. J.
Buonanno, A.
Buskulic, D.
Buy, C.
Byer, R. L.
Cadonati, L.
Cagnoli, G.
Cahillane, C.
Bustillo, J. Calderon
Callister, T.
Calloni, E.
Camp, J. B.
Cannon, K. C.
Cao, J.
Capano, C. D.
Capocasa, E.
Carbognani, F.
Caride, S.
Diaz, J. Casanueva
Casentini, C.
Caudill, S.
Cavaglia, M.
Cavalier, F.
Cavalieri, R.
Cella, G.
Cepeda, C. B.
Baiardi, L. Cerboni
Cerretani, G.
Cesarini, E.
Chakraborty, R.
Chalermsongsak, T.
Chamberlin, S. J.
Chan, M.
Chao, S.
Charlton, P.
Chassande-Mottin, E.
Chen, H. Y.
Chen, Y.
Cheng, C.
Chincarini, A.
Chiummo, A.
Cho, H. S.
Cho, M.
Chow, J. H.
Christensen, N.
Chu, Q.
Chua, S.
Chung, S.
Ciani, G.
Clara, F.
Clark, J. A.
Cleva, F.
Coccia, E.
Cohadon, P. -F.
Colla, A.
Collette, C. G.
Cominsky, L.
Constancio, M., Jr.
Conte, A.
Conti, L.
Cook, D.
Corbitt, T. R.
Cornish, N.
Corsi, A.
Cortese, S.
Costa, C. A.
Coughlin, M. W.
Coughlin, S. B.
Coulon, J. -P.
Countryman, S. T.
Couvares, P.
Cowan, E. E.
Coward, D. M.
Cowart, M. J.
Coyne, D. C.
Coyne, R.
Craig, K.
Creighton, J. D. E.
Cripe, J.
Crowder, S. G.
Cumming, A.
Cunningham, L.
Cuoco, E.
Dal Canton, T.
Danilishin, S. L.
D'Antonio, S.
Danzmann, K.
Darman, N. S.
Dattilo, V.
Dave, I.
Daveloza, H. P.
Davier, M.
Davies, G. S.
Daw, E. J.
Day, R.
DeBra, D.
Debreczeni, G.
Degallaix, J.
De Laurentis, M.
Deleglise, S.
Del Pozzo, W.
Denker, T.
Dent, T.
Dereli, H.
Dergachev, V.
DeRosa, R. T.
De Rosa, R.
DeSalvo, R.
Dhurandhar, S.
Diaz, M. C.
Di Fiore, L.
Di Giovanni, M.
Di Lieto, A.
Di Pace, S.
Di Palma, I.
Di Virgilio, A.
Dojcinoski, G.
Dolique, V.
Donovan, F.
Dooley, K. L.
Doravari, S.
Douglas, R.
Downes, T. P.
Drago, M.
Drever, R. W. P.
Driggers, J. C.
Du, Z.
Ducrot, M.
Dwyer, S. E.
Edo, T. B.
Edwards, M. C.
Effler, A.
Eggenstein, H. -B.
Ehrens, P.
Eichholz, J.
Eikenberry, S. S.
Engels, W.
Essick, R. C.
Etzel, T.
Evans, M.
Evans, T. M.
Everett, R.
Factourovich, M.
Fafone, V.
Fair, H.
Fairhurst, S.
Fan, X.
Fang, Q.
Farinon, S.
Farr, B.
Farr, W. M.
Favata, M.
Fays, M.
Fehrmann, H.
Fejer, M. M.
Ferrante, I.
Ferreira, E. C.
Ferrini, F.
Fidecaro, F.
Fiori, I.
Fiorucci, D.
Fisher, R. P.
Flaminio, R.
Fletcher, M.
Fournier, J. -D.
Franco, S.
Frasca, S.
Frasconi, F.
Frei, Z.
Freise, A.
Frey, R.
Frey, V.
Fricke, T. T.
Fritschel, P.
Frolov, V. V.
Fulda, P.
Fyffe, M.
Gabbard, H. A. G.
Gair, J. R.
Gammaitoni, L.
Gaonkar, S. G.
Garufi, F.
Gatto, A.
Gaur, G.
Gehrels, N.
Gemme, G.
Gendre, B.
Genin, E.
Gennai, A.
George, J.
Gergely, L.
Germain, V.
Ghosh, Archisman
Ghosh, S.
Giaime, J. A.
Giardina, K. D.
Giazotto, A.
Gill, K.
Glaefke, A.
Goetz, E.
Goetz, R.
Gondan, L.
Gonzalez, G.
Castro, J. M. Gonzalez
Gopakumar, A.
Gordon, N. A.
Gorodetsky, M. L.
Gossan, S. E.
Gosselin, M.
Gouaty, R.
Graef, C.
Graff, P. B.
Granata, M.
Grant, A.
Gras, S.
Gray, C.
Greco, G.
Green, A. C.
Groot, P.
Grote, H.
Grunewald, S.
Guidi, G. M.
Guo, X.
Gupta, A.
Gupta, M. K.
Gushwa, K. E.
Gustafson, E. K.
Gustafson, R.
Hacker, J. J.
Hall, B. R.
Hall, E. D.
Hammond, G.
Haney, M.
Hanke, M. M.
Hanks, J.
Hanna, C.
Hannam, M. D.
Hanson, J.
Hardwick, T.
Haris, K.
Harms, J.
Harry, G. M.
Harry, I. W.
Hart, M. J.
Hartman, M. T.
Haster, C. -J.
Haughian, K.
Heidmann, A.
Heintze, M. C.
Heitmann, H.
Hello, P.
Hemming, G.
Hendry, M.
Heng, I. S.
Hennig, J.
Heptonstall, A. W.
Heurs, M.
Hild, S.
Hoak, D.
Hodge, K. A.
Hofman, D.
Hollitt, S. E.
Holt, K.
Holz, D. E.
Hopkins, P.
Hosken, D. J.
Hough, J.
Houston, E. A.
Howell, E. J.
Hu, Y. M.
Huang, S.
Huerta, E. A.
Huet, D.
Hughey, B.
Husa, S.
Huttner, S. H.
Huynh-Dinh, T.
Idrisy, A.
Indik, N.
Ingram, D. R.
Inta, R.
Isa, H. N.
Isac, J. -M.
Isi, M.
Islas, G.
Isogai, T.
Iyer, B. R.
Izumi, K.
Jacqmin, T.
Jang, H.
Jani, K.
Jaranowski, P.
Jawahar, S.
Jimenez-Forteza, F.
Johnson, W. W.
Jones, D. I.
Jones, R.
Jonker, R. J. G.
Ju, L.
Kalaghatgi, C. V.
Kalogera, V.
Kandhasamy, S.
Kang, G.
Kanner, J. B.
Karki, S.
Kasprzack, M.
Katsavounidis, E.
Katzman, W.
Kaufer, S.
Kaur, T.
Kawabe, K.
Kawazoe, F.
Kefelian, F.
Kehl, M. S.
Keitel, D.
Kelley, D. B.
Kells, W.
Kennedy, R.
Key, J. S.
Khalaidovski, A.
Khalili, F. Y.
Khan, I.
Khan, S.
Khan, Z.
Khazanov, E. A.
Kijbunchoo, N.
Kim, C.
Kim, J.
Kim, K.
Kim, Nam-Gyu
Kim, Namjun
Kim, Y. -M.
King, E. J.
King, P. J.
Kinzel, D. L.
Kissel, J. S.
Kleybolte, L.
Klimenko, S.
Koehlenbeck, S. M.
Kokeyama, K.
Koley, S.
Kondrashov, V.
Kontos, A.
Korobko, M.
Korth, W. Z.
Kowalska, I.
Kozak, D. B.
Kringel, V.
Krolak, A.
Krueger, C.
Kuehn, G.
Kumar, P.
Kuo, L.
Kutynia, A.
Lackey, B. D.
Landry, M.
Lange, J.
Lantz, B.
Lasky, P. D.
Lazzarini, A.
Lazzaro, C.
Leaci, P.
Leavey, S.
Lebigot, E. O.
Lee, C. H.
Lee, H. K.
Lee, H. M.
Lee, K.
Lenon, A.
Leonardi, M.
Leong, J. R.
Leroy, N.
Letendre, N.
Levin, Y.
Levine, B. M.
Li, T. G. F.
Libson, A.
Littenberg, T. B.
Lockerbie, N. A.
Logue, J.
Lombardi, A. L.
Lord, J. E.
Lorenzini, M.
Loriette, V.
Lormand, M.
Losurdo, G.
Lough, J. D.
Lueck, H.
Lundgren, A. P.
Luo, J.
Lynch, R.
Ma, Y.
MacDonald, T.
Machenschalk, B.
MacInnis, M.
Macleod, D. M.
Magana-Sandoval, F.
Magee, R. M.
Mageswaran, M.
Majorana, E.
Maksimovic, I.
Malvezzi, V.
Man, N.
Mandel, I.
Mandic, V.
Mangano, V.
Mansell, G. L.
Manske, M.
Mantovani, M.
Marchesoni, F.
Marion, F.
Marka, S.
Marka, Z.
Markosyan, A. S.
Maros, E.
Martelli, F.
Martellini, L.
Martin, I. W.
Martin, R. M.
Martynov, D. V.
Marx, J. N.
Mason, K.
Masserot, A.
Massinger, T. J.
Masso-Reid, M.
Matichard, F.
Matone, L.
Mavalvala, N.
Mazumder, N.
Mazzolo, G.
McCarthy, R.
McClelland, D. E.
McCormick, S.
McGuire, S. C.
McIntyre, G.
McIver, J.
McManus, D. J.
McWilliams, S. T.
Meacher, D.
Meadors, G. D.
Meidam, J.
Melatos, A.
Mendell, G.
Mendoza-Gandara, D.
Mercer, R. A.
Merilh, E.
Merzougui, M.
Meshkov, S.
Messenger, C.
Messick, C.
Meyers, P. M.
Mezzani, F.
Miao, H.
Michel, C.
Middleton, H.
Mikhailov, E. E.
Milano, L.
Miller, J.
Millhouse, M.
Minenkov, Y.
Ming, J.
Mirshekari, S.
Mishra, C.
Mitra, S.
Mitrofanov, V. P.
Mitselmakher, G.
Mittleman, R.
Moggi, A.
Mohan, M.
Mohapatra, S. R. P.
Montani, M.
Moore, B. C.
Moore, C. J.
Moraru, D.
Moreno, G.
Morriss, S. R.
Mossavi, K.
Mours, B.
Mow-Lowry, C. M.
Mueller, C. L.
Mueller, G.
Muir, A. W.
Mukherjee, Arunava
Mukherjee, D.
Mukherjee, S.
Mukund, N.
Mullavey, A.
Munch, J.
Murphy, D. J.
Murray, P. G.
Mytidis, A.
Nardecchia, I.
Naticchioni, L.
Nayak, R. K.
Necula, V.
Nedkova, K.
Nelemans, G.
Neri, M.
Neunzert, A.
Newton, G.
Nguyen, T. T.
Nielsen, A. B.
Nissanke, S.
Nitz, A.
Nocera, F.
Nolting, D.
Normandin, M. E. N.
Nuttall, L. K.
Oberling, J.
Ochsner, E.
O'Dell, J.
Oelker, E.
Ogin, G. H.
Oh, J. J.
Oh, S. H.
Ohme, F.
Oliver, M.
Oppermann, P.
Oram, Richard J.
O'Reilly, B.
O'Shaughnessy, R.
Ottaway, D. J.
Ottens, R. S.
Overmier, H.
Owen, B. J.
Pai, A.
Pai, S. A.
Palamos, J. R.
Palashov, O.
Palomba, C.
Pal-Singh, A.
Pan, H.
Pankow, C.
Pannarale, F.
Pant, B. C.
Paoletti, F.
Paoli, A.
Papa, M. A.
Paris, H. R.
Parker, W.
Pascucci, D.
Pasqualetti, A.
Passaquieti, R.
Passuello, D.
Patricelli, B.
Patrick, Z.
Pearlstone, B. L.
Pedraza, M.
Pedurand, R.
Pekowsky, L.
Pele, A.
Penn, S.
Perreca, A.
Phelps, M.
Piccinni, O.
Pichot, M.
Piergiovanni, F.
Pierro, V.
Pillant, G.
Pinard, L.
Pinto, I. M.
Pitkin, M.
Poggiani, R.
Popolizio, P.
Post, A.
Powell, J.
Prasad, J.
Predoi, V.
Premachandra, S. S.
Prestegard, T.
Price, L. R.
Prijatelj, M.
Principe, M.
Privitera, S.
Prodi, G. A.
Prokhorov, L.
Puncken, O.
Punturo, M.
Puppo, P.
Puerrer, M.
Qi, H.
Qin, J.
Quetschke, V.
Quintero, E. A.
Quitzow-James, R.
Raab, F. J.
Rabeling, D. S.
Radkins, H.
Raffai, P.
Raja, S.
Rakhmanov, M.
Rapagnani, P.
Raymond, V.
Razzano, M.
Re, V.
Read, J.
Reed, C. M.
Regimbau, T.
Rei, L.
Reid, S.
Reitze, D. H.
Rew, H.
Reyes, S. D.
Ricci, F.
Riles, K.
Robertson, N. A.
Robie, R.
Robinet, F.
Rocchi, A.
Rolland, L.
Rollins, J. G.
Roma, V. J.
Romano, J. D.
Romano, R.
Romanov, G.
Romie, J. H.
Rosinska, D.
Rowan, S.
Ruediger, A.
Ruggi, P.
Ryan, K.
Sachdev, S.
Sadecki, T.
Sadeghian, L.
Salconi, L.
Saleem, M.
Salemi, F.
Samajdar, A.
Sammut, L.
Sanchez, E. J.
Sandberg, V.
Sandeen, B.
Sanders, J. R.
Sassolas, B.
Sathyaprakash, B. S.
Saulson, P. R.
Sauter, O.
Savage, R. L.
Sawadsky, A.
Schale, P.
Schilling, R.
Schmidt, J.
Schmidt, P.
Schnabel, R.
Schofield, R. M. S.
Schoenbeck, A.
Schreiber, E.
Schuette, D.
Schutz, B. F.
Scott, J.
Scott, S. M.
Sellers, D.
Sentenac, D.
Sequino, V.
Sergeev, A.
Serna, G.
Setyawati, Y.
Sevigny, A.
Shaddock, D. A.
Shah, S.
Shahriar, M. S.
Shaltev, M.
Shao, Z.
Shapiro, B.
Shawhan, P.
Sheperd, A.
Shoemaker, D. H.
Shoemaker, D. M.
Siellez, K.
Siemens, X.
Sigg, D.
Silva, A. D.
Simakov, D.
Singer, A.
Singer, L. P.
Singh, A.
Singh, R.
Singhal, A.
Sintes, A. M.
Slagmolen, B. J. J.
Smith, J. R.
Smith, N. D.
Smith, R. J. E.
Son, E. J.
Sorazu, B.
Sorrentino, F.
Souradeep, T.
Srivastava, A. K.
Staley, A.
Steinke, M.
Steinlechner, J.
Steinlechner, S.
Steinmeyer, D.
Stephens, B. C.
Stone, R.
Strain, K. A.
Straniero, N.
Stratta, G.
Strauss, N. A.
Strigin, S.
Sturani, R.
Stuver, A. L.
Summerscales, T. Z.
Sun, L.
Sutton, P. J.
Swinkels, B. L.
Szczepanczyk, M. J.
Tacca, M.
Talukder, D.
Tanner, D. B.
Tapai, M.
Tarabrin, S. P.
Taracchini, A.
Taylor, R.
Theeg, T.
Thirugnanasambandam, M. P.
Thomas, E. G.
Thomas, M.
Thomas, P.
Thorne, K. A.
Thorne, K. S.
Thrane, E.
Tiwari, S.
Tiwari, V.
Tokmakov, K. V.
Tomlinson, C.
Tonelli, M.
Torres, C. V.
Torrie, C. I.
Toeyrae, D.
Travasso, F.
Traylor, G.
Trifiro, D.
Tringali, M. C.
Trozzo, L.
Tse, M.
Turconi, M.
Tuyenbayev, D.
Ugolini, D.
Unnikrishnan, C. S.
Urban, A. L.
Usman, S. A.
Vahlbruch, H.
Vajente, G.
Valdes, G.
Van Bakel, N.
Van Beuzekom, M.
Van den Brand, J. F. J.
Van den Broeck, C.
Vander-Hyde, D. C.
Van der Schaaf, L.
van Heijningen, J. V.
van Veggel, A. A.
Vardaro, M.
Vass, S.
Vasuth, M.
Vaulin, R.
Vecchio, A.
Vedovato, G.
Veitch, J.
Veitch, P. J.
Venkateswara, K.
Verkindt, D.
Vetrano, F.
Vicere, A.
Vinciguerra, S.
Vine, D. J.
Vinet, J. -Y.
Vitale, S.
Vo, T.
Vocca, H.
Vorvick, C.
Voss, D.
Vousden, W. D.
Vyatchanin, S. P.
Wade, A. R.
Wade, L. E.
Wade, M.
Walker, M.
Wallace, L.
Walsh, S.
Wang, G.
Wang, H.
Wang, M.
Wang, X.
Wang, Y.
Ward, R. L.
Warner, J.
Was, M.
Weaver, B.
Wei, L. -W.
Weinert, M.
Weinstein, A. J.
Weiss, R.
Welborn, T.
Wen, L.
Wessels, P.
Westphal, T.
Wette, K.
Whelan, J. T.
White, D. J.
Whiting, B. F.
Williams, R. D.
Williamson, A. R.
Willis, J. L.
Willke, B.
Wimmer, M. H.
Winkler, W.
Wipf, C. C.
Wittel, H.
Woan, G.
Worden, J.
Wright, J. L.
Wu, G.
Yablon, J.
Yam, W.
Yamamoto, H.
Yancey, C. C.
Yap, M. J.
Yu, H.
Yvert, M.
Zadrozny, A.
Zangrando, L.
Zanolin, M.
Zendri, J. -P.
Zevin, M.
Zhang, F.
Zhang, L.
Zhang, M.
Zhang, Y.
Zhao, C.
Zhou, M.
Zhou, Z.
Zhu, X. J.
Zucker, M. E.
Zuraw, S. E.
Zweizig, J.
CA LIGO Sci Collaboration
Virgo Collaboration
TI GW150914: Implications for the Stochastic Gravitational-Wave Background
from Binary Black Holes
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID GAMMA-RAY BURSTS; STAR-FORMATION; HIGH-REDSHIFT; COALESCENCE RATES;
MERGER RATES; EVOLUTION; INTERFEROMETERS; POPULATION; ORIGIN
AB The LIGO detection of the gravitational wave transient GW150914, from the inspiral and merger of two black holes with masses >= 30M(circle dot), suggests a population of binary black holes with relatively high mass. This observation implies that the stochastic gravitational-wave background from binary black holes, created from the incoherent superposition of all the merging binaries in the Universe, could be higher than previously expected. Using the properties of GW150914, we estimate the energy density of such a background from binary black holes. In the most sensitive part of the Advanced LIGO and Advanced Virgo band for stochastic backgrounds (near 25 Hz), we predict Omega(GW)(f = 25 Hz) = 1.1(-0.9) (+2.7) x 10(-9) with 90% confidence. This prediction is robustly demonstrated for a variety of formation scenarios with different parameters. The differences between models are small compared to the statistical uncertainty arising from the currently poorly constrained local coalescence rate. We conclude that this background is potentially measurable by the Advanced LIGO and Advanced Virgo detectors operating at their projected final sensitivity.
C1 [Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Anderson, S. B.; Arai, K.; Araya, M. C.; Barayoga, J. C.; Barish, B. C.; Berger, B. K.; Billingsley, G.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cahillane, C.; Callister, T.; Cepeda, C. B.; Chakraborty, R.; Chalermsongsak, T.; Couvares, P.; Coyne, D. C.; Dergachev, V.; Drever, R. W. P.; Ehrens, P.; Etzel, T.; Gossan, S. E.; Gushwa, K. E.; Gustafson, E. K.; Hall, E. D.; Heptonstall, A. W.; Hodge, K. A.; Isi, M.; Kanner, J. B.; Kells, W.; Kondrashov, V.; Korth, W. Z.; Kozak, D. B.; Lazzarini, A.; Li, T. G. F.; Mageswaran, M.; Maros, E.; Martynov, D. V.; Marx, J. N.; McIntyre, G.; McIver, J.; Meshkov, S.; Pedraza, M.; Perreca, A.; Price, L. R.; Quintero, E. A.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sachdev, S.; Sanchez, E. J.; Schmidt, P.; Shao, Z.; Singer, A.; Smith, N. D.; Smith, R. J. E.; Taylor, R.; Thirugnanasambandam, M. P.; Torrie, C. I.; Vajente, G.; Vass, S.; Wallace, L.; Weinstein, A. J.; Williams, R. D.; Wipf, C. C.; Yamamoto, H.; Zhang, L.; Zucker, M. E.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Abbott, T. D.; Buchanan, C. C.; Corbitt, T. R.; Cripe, J.; Giaime, J. A.; Gonzalez, G.; Hardwick, T.; Johnson, W. W.; Kasprzack, M.; Kokeyama, K.; Macleod, D. M.; Singh, R.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Acernese, F.; Addesso, P.; Barone, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy.
[Acernese, F.; Barone, F.; Calloni, E.; De Laurentis, M.; De Rosa, R.; Di Fiore, L.; Garufi, F.; Milano, L.; Romano, R.] Ist Nazl Fis Nucl, Sez Napoli, Complesso Univ Monte St Angelo, I-80126 Naples, Italy.
[Ackley, K.; Ciani, G.; Eichholz, J.; Eikenberry, S. S.; Fulda, P.; Goetz, R.; Hartman, M. T.; Heintze, M. C.; Klimenko, S.; Martin, R. M.; Mitselmakher, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Necula, V.; Ottens, R. S.; Reitze, D. H.; Tanner, D. B.; Voss, D.; Whiting, B. F.] Univ Florida, Gainesville, FL 32611 USA.
[Adams, C.; Aston, S. M.; Betzwieser, J.; Birch, J.; Cowart, M. J.; DeRosa, R. T.; Doravari, S.; Effler, A.; Evans, T. M.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hanson, J.; Heintze, M. C.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Kinzel, D. L.; Lormand, M.; McCormick, S.; Mullavey, A.; Nolting, D.; Oram, Richard J.; O'Reilly, B.; Overmier, H.; Parker, W.; Pele, A.; Romie, J. H.; Sellers, D.; Stuver, A. L.; Thomas, M.; Thorne, K. A.; Traylor, G.; Welborn, T.; Wu, G.] LIGO Livingston Observ, Livingston, LA 70754 USA.
[Adams, T.; Bonnand, R.; Buskulic, D.; Ducrot, M.; Germain, V.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Verkindt, D.; Was, M.; Yvert, M.] Univ Savoie Mt Blanc, CNRS IN2P3, LAPP, F-74941 Annecy Le Vieux, France.
[Adya, V. B.; Affeldt, C.; Allen, B.; Aufmuth, P.; Aulbert, C.; Baune, C.; Bergmann, G.; Bisht, A.; Bock, O.; Bogan, C.; Brinkmann, M.; Capano, C. D.; Dal Canton, T.; Danzmann, K.; Denker, T.; Dent, T.; Di Palma, I.; Doravari, S.; Drago, M.; Eggenstein, H. -B.; Fehrmann, H.; Fricke, T. T.; Grote, H.; Hanke, M. M.; Heurs, M.; Indik, N.; Kawazoe, F.; Keitel, D.; Khalaidovski, A.; Koehlenbeck, S. M.; Kringel, V.; Kuehn, G.; Leong, J. R.; Lough, J. D.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Mazzolo, G.; Meadors, G. D.; Mendoza-Gandara, D.; Ming, J.; Mossavi, K.; Nielsen, A. B.; Nitz, A.; Oppermann, P.; Papa, M. A.; Post, A.; Puncken, O.; Ruediger, A.; Salemi, F.; Schilling, R.; Schmidt, J.; Schreiber, E.; Schuette, D.; Shaltev, M.; Simakov, D.; Singh, A.; Steinke, M.; Steinmeyer, D.; Tarabrin, S. P.; Theeg, T.; Walsh, S.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Whelan, J. T.; Willke, B.; Wimmer, M. H.; Winkler, W.; Wittel, H.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Agathos, M.; Agatsuma, K.; Bader, M. K. M.; Bertolini, A.; Boom, B. A.; Bulten, H. J.; Ghosh, S.; Jonker, R. J. G.; Koley, S.; Meidam, J.; Nelemans, G.; Nissanke, S.; Setyawati, Y.; Shah, S.; Van Bakel, N.; Van Beuzekom, M.; Van den Brand, J. F. J.; Van den Broeck, C.; Van der Schaaf, L.; van Heijningen, J. V.] Nikhef, Sci Pk, NL-1098 XG Amsterdam, Netherlands.
[Aggarwal, N.; Barsotti, L.; Biscans, S.; Bodiya, T. P.; Brown, N. M.; Buikema, A.; Donovan, F.; Essick, R. C.; Evans, M.; Fritschel, P.; Gras, S.; Isogai, T.; Katsavounidis, E.; Kontos, A.; Libson, A.; Lynch, R.; MacInnis, M.; Mason, K.; Matichard, F.; Mavalvala, N.; Miller, J.; Mittleman, R.; Mohapatra, S. R. P.; Oelker, E.; Shoemaker, D. H.; Tse, M.; Vaulin, R.; Vitale, S.; Weiss, R.; Yam, W.; Yu, H.; Zhang, F.; Zucker, M. E.] MIT, LIGO, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Aguiar, O. D.; Constancio, M., Jr.; Costa, C. A.; Ferreira, E. C.; Silva, A. D.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Paulo, Brazil.
[Aiello, L.; Coccia, E.; Fafone, V.; Khan, I.; Lorenzini, M.; Singhal, A.; Tiwari, S.; Wang, G.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy.
[Aiello, L.; Ascenzi, S.; Casentini, C.; Cesarini, E.; Coccia, E.; D'Antonio, S.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Minenkov, Y.; Nardecchia, I.; Rocchi, A.; Sequino, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Ain, A.; Bose, S.; Dhurandhar, S.; Gaonkar, S. G.; Gupta, A.; Mitra, S.; Mukund, N.; Prasad, J.; Souradeep, T.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Ajith, P.; Ghosh, Archisman; Iyer, B. R.; Mishra, C.; Mukherjee, Arunava] Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bangalore 560012, Karnataka, India.
[Allen, B.; Anderson, W. G.; Brady, P. R.; Brockill, P.; Caudill, S.; Creighton, J. D. E.; Downes, T. P.; Manske, M.; Mercer, R. A.; Mukherjee, D.; Ochsner, E.; Papa, M. A.; Qi, H.; Sadeghian, L.; Sheperd, A.; Siemens, X.; Stephens, B. C.; Urban, A. L.; Walsh, S.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Allen, B.; Bisht, A.; Danzmann, K.; Denker, T.; Heurs, M.; Kaufer, S.; Kawazoe, F.; Krueger, C.; Lough, J. D.; Lueck, H.; Sawadsky, A.; Schuette, D.; Steinmeyer, D.; Vahlbruch, H.; Willke, B.; Wimmer, M. H.; Wittel, H.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Allocca, A.; Basti, A.; Boschi, V.; Cerretani, G.; Di Lieto, A.; Ferrante, I.; Fidecaro, F.; Castro, J. M. Gonzalez; Passaquieti, R.; Patricelli, B.; Poggiani, R.; Razzano, M.; Tonelli, M.] Univ Pisa, I-56127 Pisa, Italy.
[Allocca, A.; Basti, A.; Boschi, V.; Bradaschia, C.; Cella, G.; Cerretani, G.; Di Lieto, A.; Di Virgilio, A.; Ferrante, I.; Fidecaro, F.; Frasconi, F.; Gennai, A.; Giazotto, A.; Castro, J. M. Gonzalez; Moggi, A.; Paoletti, F.; Passaquieti, R.; Passuello, D.; Patricelli, B.; Poggiani, R.; Razzano, M.; Tonelli, M.; Trozzo, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Altin, P. A.; Chow, J. H.; Mansell, G. L.; McClelland, D. E.; McManus, D. J.; Nguyen, T. T.; Rabeling, D. S.; Scott, S. M.; Shaddock, D. A.; Slagmolen, B. J. J.; Wade, A. R.; Ward, R. L.; Yap, M. J.] Australian Natl Univ, GPO Box 4, Canberra, ACT 0200, Australia.
[Arceneaux, C. C.; Cavaglia, M.; Dooley, K. L.; Gabbard, H. A. G.; Kandhasamy, S.; Trifiro, D.] Univ Mississippi, University, MS 38677 USA.
[Areeda, J. S.; Hacker, J. J.; Islas, G.; Read, J.; Serna, G.; Smith, J. R.; Vander-Hyde, D. C.] Calif State Univ Fullerton, Fullerton, CA 92831 USA.
[Arnaud, N.; Bizouard, M. A.; Brisson, V.; Diaz, J. Casanueva; Cavalier, F.; Davier, M.; Franco, S.; Frey, V.; Hello, P.; Huet, D.; Kasprzack, M.; Leroy, N.; Robinet, F.] Univ Paris Saclay, Univ Paris Sud, CNRS IN2P3, Lab Accelerateur Lineaire, BP 34, F-91898 Orsay, France.
[Arun, K. G.; Kalaghatgi, C. V.] Chennai Math Inst, Siruseri 603103, India.
[Ascenzi, S.; Casentini, C.; Cesarini, E.; Coccia, E.; Fafone, V.; Malvezzi, V.; Nardecchia, I.; Re, V.; Sequino, V.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Ashton, G.; Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Ast, M.; Kleybolte, L.; Korobko, M.; Pal-Singh, A.; Schnabel, R.; Schoenbeck, A.] Univ Hamburg, D-22761 Hamburg, Germany.
[Astone, P.; Colla, A.; Conte, A.; Di Giovanni, M.; Di Pace, S.; Frasca, S.; Leaci, P.; Majorana, E.; Mezzani, F.; Naticchioni, L.; Palomba, C.; Piccinni, O.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
[Babak, S.; Behnke, B.; Bohe, A.; Buonanno, A.; Di Palma, I.; Grunewald, S.; Harry, I. W.; Leaci, P.; Meadors, G. D.; Ming, J.; Papa, M. A.; Privitera, S.; Puerrer, M.; Raymond, V.; Schutz, B. F.; Singh, A.; Taracchini, A.; Walsh, S.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany.
[Bacon, P.; Barsuglia, M.; Bouffanais, Y.; Buy, C.; Capocasa, E.; Chassande-Mottin, E.; Fiorucci, D.; Gatto, A.; Lebigot, E. O.; Tacca, M.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, APC,Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France.
[Baker, P. T.; Cornish, N.; Millhouse, M.] Montana State Univ, Bozeman, MT 59717 USA.
[Baldaccini, F.; Gammaitoni, L.; Travasso, F.; Vocca, H.] Univ Perugia, I-06123 Perugia, Italy.
[Baldaccini, F.; Gammaitoni, L.; Marchesoni, F.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Ballardin, G.; Bavigadda, V.; Bitossi, M.; Bozzi, A.; Carbognani, F.; Cavalieri, R.; Chiummo, A.; Cortese, S.; Cuoco, E.; Dattilo, V.; Day, R.; Ferrini, F.; Fiori, I.; Genin, E.; Gosselin, M.; Hemming, G.; Kasprzack, M.; Mantovani, M.; Mohan, M.; Nocera, F.; Paoletti, F.; Paoli, A.; Pasqualetti, A.; Pillant, G.; Popolizio, P.; Prijatelj, M.; Ruggi, P.; Salconi, L.; Sentenac, D.; Swinkels, B. L.] EGO, I-56021 Pisa, Italy.
[Ballmer, S. W.; Bhagwat, S.; Biwer, C.; Fair, H.; Fisher, R. P.; Kelley, D. B.; Lackey, B. D.; Lenon, A.; Lord, J. E.; Magana-Sandoval, F.; Massinger, T. J.; Nuttall, L. K.; Pekowsky, L.; Reyes, S. D.; Sanders, J. R.; Saulson, P. R.; Usman, S. A.; Vander-Hyde, D. C.; Vo, T.] Syracuse Univ, Syracuse, NY 13244 USA.
[Barclay, S. E.; Barr, B.; Bell, A. S.; Bell, C. J.; Chan, M.; Craig, K.; Cumming, A.; Cunningham, L.; Danilishin, S. L.; Davies, G. S.; Douglas, R.; Fletcher, M.; Glaefke, A.; Gordon, N. A.; Graef, C.; Grant, A.; Hammond, G.; Hart, M. J.; Haughian, K.; Hendry, M.; Heng, I. S.; Hennig, J.; Hild, S.; Hough, J.; Houston, E. A.; Hu, Y. M.; Huttner, S. H.; Isa, H. N.; Jones, R.; Leavey, S.; Lee, K.; Logue, J.; Mangano, V.; Martin, I. W.; Masso-Reid, M.; Messenger, C.; Murray, P. G.; Newton, G.; Pascucci, D.; Pearlstone, B. L.; Phelps, M.; Pitkin, M.; Powell, J.; Robertson, N. A.; Robie, R.; Rowan, S.; Scott, J.; Sorazu, B.; Steinlechner, J.; Steinlechner, S.; Strain, K. A.; van Veggel, A. A.; Woan, G.; Wright, J. L.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Barker, D.; Bartlett, J.; Batch, J. C.; Bergman, J.; Blair, M.; Clara, F.; Cook, D.; Driggers, J. C.; Dwyer, S. E.; Gray, C.; Hanks, J.; Ingram, D. R.; Izumi, K.; Kawabe, K.; Kijbunchoo, N.; King, P. J.; Kissel, J. S.; Landry, M.; Levine, B. M.; McCarthy, R.; Mendell, G.; Merilh, E.; Moraru, D.; Moreno, G.; Oberling, J.; Raab, F. J.; Radkins, H.; Reed, C. M.; Ryan, K.; Sadecki, T.; Sandberg, V.; Savage, R. L.; Sevigny, A.; Sigg, D.; Thomas, P.; Vorvick, C.; Warner, J.; Weaver, B.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA.
[Barta, D.; Debreczeni, G.; Vasuth, M.] RMKI, Wigner RCP, Konkoly Thege Miklos Ut 29-33, H-1121 Budapest, Hungary.
[Bartos, I.; Countryman, S. T.; Factourovich, M.; Marka, S.; Marka, Z.; Matone, L.; Murphy, D. J.; Staley, A.] Columbia Univ, New York, NY 10027 USA.
[Bassiri, R.; Byer, R. L.; DeBra, D.; Fejer, M. M.; Kim, Namjun; Lantz, B.; MacDonald, T.; Markosyan, A. S.; Paris, H. R.; Patrick, Z.; Shapiro, B.] Stanford Univ, Stanford, CA 94305 USA.
[Bazzan, M.; Vardaro, M.] Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy.
[Bazzan, M.; Conti, L.; Lazzaro, C.; Vardaro, M.; Vedovato, G.; Zangrando, L.; Zendri, J. -P.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bejger, M.; Rosinska, D.] CAMK PAN, PL-00716 Warsaw, Poland.
[Bulik, T.; Kowalska, I.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
[Berry, C. P. L.; Bond, C.; Brown, D. D.; Del Pozzo, W.; Farr, W. M.; Freise, A.; Green, A. C.; Haster, C. -J.; Mandel, I.; Miao, H.; Middleton, H.; Mow-Lowry, C. M.; Thomas, E. G.; Toeyrae, D.; Vecchio, A.; Veitch, J.; Vinciguerra, S.; Vousden, W. D.; Wang, H.; Wang, M.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Bersanetti, D.; Neri, M.] Univ Genoa, I-16146 Genoa, Italy.
[Bersanetti, D.; Chincarini, A.; Farinon, S.; Gemme, G.; Neri, M.; Rei, L.; Sorrentino, F.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy.
[Bhandare, R.; Dave, I.; George, J.; Pai, S. A.; Pant, B. C.; Raja, S.] RRCAT, Indore 452013, Madhya Pradesh, India.
[Bilenko, I. A.; Braginsky, V. B.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L.; Strigin, S.; Vyatchanin, S. P.] Moscow MV Lomonosov State Univ, Fac Phys, Moscow 119991, Russia.
[Birney, R.; Reid, S.; Vine, D. J.] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland.
[Blair, C. D.; Blair, D. G.; Chu, Q.; Chung, S.; Coward, D. M.; Fang, Q.; Howell, E. J.; Ju, L.; Kaur, T.; Ma, Y.; Qin, J.; Wang, Y.; Wen, L.; Zhao, C.; Zhu, X. J.] Univ Western Australia, Crawley, WA 6009, Australia.
[Bloemen, S.; Ghosh, S.; Groot, P.; Nelemans, G.; Nissanke, S.; Setyawati, Y.; Shah, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Baldaccini, F.; Gammaitoni, L.; Marchesoni, F.; Punturo, M.; Travasso, F.; Vocca, H.] Univ Cote dAzur, CNRS, Artemis Observ Cote dAzur, CS 34229, F-06304 Nice 4, France.
[Bojtos, P.; Frei, Z.; Gondan, L.; Raffai, P.] MTA Eotvos Univ, Lendulet Astrophys Res Grp, H-1117 Budapest, Hungary.
[Bondu, F.] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France.
[Bose, S.; Hall, B. R.; Magee, R. M.; Mazumder, N.] Washington State Univ, Pullman, WA 99164 USA.
[Branchesi, M.; Baiardi, L. Cerboni; Greco, G.; Guidi, G. M.; Harms, J.; Martelli, F.; Montani, M.; Piergiovanni, F.; Stratta, G.; Vetrano, F.; Vicere, A.] Univ Urbino Carlo Bo, I-61029 Urbino, Italy.
[Branchesi, M.; Baiardi, L. Cerboni; Greco, G.; Guidi, G. M.; Harms, J.; Losurdo, G.; Martelli, F.; Montani, M.; Piergiovanni, F.; Stratta, G.; Vetrano, F.; Vicere, A.] Ist Nazl Fis Nucl, Sez Firenze, I-50125 Florence, Italy.
[Brau, J. E.; Frey, R.; Karki, S.; Palamos, J. R.; Quitzow-James, R.; Roma, V. J.; Schale, P.; Schofield, R. M. S.; Talukder, D.] Univ Oregon, Eugene, OR 97403 USA.
[Briant, T.; Chua, S.; Cohadon, P. -F.; Deleglise, S.; Heidmann, A.; Isac, J. -M.; Jacqmin, T.] Univ Paris 06, Sorbonne Univ, ENS PSL Res Univ, Lab Kastler Brossel,CNRS,Coll France, F-75005 Paris, France.
[Bulten, H. J.; Van den Brand, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands.
[Buonanno, A.; Cho, M.; Graff, P. B.; Shawhan, P.; Yancey, C. C.] Univ Maryland, College Pk, MD 20742 USA.
[Cadonati, L.; Bustillo, J. Calderon; Clark, J. A.; Cowan, E. E.; Jani, K.; Lazzaro, C.; Shoemaker, D. M.; Siellez, K.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Cadonati, L.; Bustillo, J. Calderon; Clark, J. A.; Cowan, E. E.; Jani, K.; Lazzaro, C.; Shoemaker, D. M.; Siellez, K.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Cagnoli, G.] Univ Lyon 1, Inst Lumiere Mat, UMR CNRS 5306, F-69622 Villeurbanne, France.
[Cagnoli, G.; Degallaix, J.; Dolique, V.; Flaminio, R.; Granata, M.; Hofman, D.; Michel, C.; Pedurand, R.; Pinard, L.; Sassolas, B.; Straniero, N.] Univ Lyon, IN2P3 CNRS, LMA, F-69622 Villeurbanne, Lyon, France.
[Bustillo, J. Calderon; Husa, S.; Jimenez-Forteza, F.; Keitel, D.; Oliver, M.; Sintes, A. M.] Univ Illes Balears, IEEC IAC3, E-07122 Palma De Mallorca, Spain.
[Calloni, E.; De Laurentis, M.; De Rosa, R.; Garufi, F.; Milano, L.] Univ Naples Federico II, Complesso Univ Monte St Angelo, I-80126 Naples, Italy.
[Camp, J. B.; Gehrels, N.; Singer, L. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cannon, K. C.; Kehl, M. S.; Kumar, P.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Cao, J.; Du, Z.; Fan, X.; Guo, X.; Lebigot, E. O.; Wang, X.] Tsinghua Univ, Beijing 100084, Peoples R China.
[Caride, S.; Corsi, A.; Coyne, R.; Inta, R.; Owen, B. J.] Texas Tech Univ, Lubbock, TX 79409 USA.
[Chamberlin, S. J.; Everett, R.; Hanna, C.; Idrisy, A.; Meacher, D.; Messick, C.] Penn State Univ, University Pk, PA 16802 USA.
[Chao, S.; Cheng, C.; Huang, S.; Kuo, L.; Pan, H.] Natl Tsing Hua Univ, Hsinchu 30013, Taiwan.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Chen, H. Y.; Farr, B.; Holz, D. E.] Univ Chicago, Chicago, IL 60637 USA.
[Chen, Y.; Engels, W.; Schmidt, P.; Thorne, K. S.] Caltech CaRT, Pasadena, CA 91125 USA.
[Cho, H. S.; Jang, H.; Kang, G.; Kim, C.; Kim, Nam-Gyu] Korea Inst Sci & Technol Informat, Daejeon 305806, South Korea.
[Christensen, N.; Coughlin, M. W.; Edwards, M. C.; Luo, J.; Strauss, N. A.] Carleton Coll, Northfield, MN 55057 USA.
[Colla, A.; Conte, A.; Di Giovanni, M.; Di Pace, S.; Frasca, S.; Leaci, P.; Mezzani, F.; Naticchioni, L.; Piccinni, O.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, Piazzale Aldo Moro 5, I-00185 Rome, Italy.
[Collette, C. G.] Univ Brussels, B-1050 Brussels, Belgium.
[Cominsky, L.] Sonoma State Univ, Rohnert Pk, CA 94928 USA.
[Coughlin, S. B.; Huerta, E. A.; Kalogera, V.; Pankow, C.; Sandeen, B.; Shahriar, M. S.; Yablon, J.; Zevin, M.; Zhou, M.; Zhou, Z.] Northwestern Univ, Evanston, IL 60208 USA.
[Crowder, S. G.; Mandic, V.; Meyers, P. M.; Prestegard, T.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Darman, N. S.; Melatos, A.; Sammut, L.; Sun, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
[Daveloza, H. P.; Diaz, M. C.; Key, J. S.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E. N.; Quetschke, V.; Rakhmanov, M.; Romano, J. D.; Stone, R.; Torres, C. V.; Tuyenbayev, D.; Valdes, G.] Univ Texas Rio Grande Valley, Brownsville, TX 78520 USA.
[Daw, E. J.; Edo, T. B.; Kennedy, R.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Ist Nazl Fis Nucl, Sez Napoli, I-80100 Naples, Italy.
[Dojcinoski, G.; Favata, M.; Moore, B. C.] Montclair State Univ, Montclair, NJ 07043 USA.
[Drago, M.; Leonardi, M.; Prodi, G. A.; Tringali, M. C.] Univ Trento, Dipartimento Fis, I-38123 Povo, Trento, Italy.
[Drago, M.; Leonardi, M.; Prodi, G. A.; Tringali, M. C.] Ist Nazl Fis Nucl, Trento Inst Fundamental Phys & Applicat, I-38123 Povo, Trento, Italy.
[Fairhurst, S.; Fays, M.; Hannam, M. D.; Hopkins, P.; Kalaghatgi, C. V.; Khan, S.; Muir, A. W.; Ohme, F.; Pannarale, F.; Predoi, V.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Tiwari, V.; Williamson, A. R.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Flaminio, R.] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Gair, J. R.] Univ Edinburgh, Sch Math, Edinburgh EH9 3FD, Midlothian, Scotland.
[Gaur, G.] Indian Inst Technol, Gandhinagar Ahmedabad 382424, Gujarat, India.
[Gaur, G.; Gupta, M. K.; Khan, Z.; Srivastava, A. K.] Inst Plasma Res, Bhat 382428, Gandhinagar, India.
[Gergely, L.; Tapai, M.] Univ Szeged, Dom Ter 9, H-6720 Szeged, Hungary.
[Gill, K.; Hughey, B.; Szczepanczyk, M. J.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Goetz, E.; Gustafson, R.; Neunzert, A.; Riles, K.; Sanders, J. R.; Sauter, O.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Gopakumar, A.; Haney, M.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India.
[Harry, G. M.] Amer Univ, Washington, DC 20016 USA.
[Hoak, D.; Lombardi, A. L.; Nedkova, K.; Zuraw, S. E.] Univ Massachusetts, Amherst, MA 01003 USA.
[Hollitt, S. E.; Hosken, D. J.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Huerta, E. A.; McWilliams, S. T.] W Virginia Univ, Morgantown, WV 26506 USA.
[Jaranowski, P.] Univ Bial Ystok, PL-15424 Bialystok, Poland.
[Jawahar, S.; Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
[Haris, K.; Pai, A.; Saleem, M.] IISER TVM, CET Campus, Trivandrum 695016, Kerala, India.
[Khazanov, E. A.; Palashov, O.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Kim, J.; Kim, Y. -M.; Lee, C. H.] Pusan Natl Univ, Busan 609735, South Korea.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Krolak, A.; Kutynia, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Lange, J.; O'Shaughnessy, R.; Whelan, J. T.; Zhang, Y.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Lasky, P. D.; Levin, Y.; Premachandra, S. S.; Sammut, L.; Thrane, E.] Monash Univ, Clayton, Vic 3800, Australia.
[Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Littenberg, T. B.] Univ Alabama, Huntsville, AL 35899 USA.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy.
[McGuire, S. C.] Southern Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.] A&M Coll, Baton Rouge, LA 70813 USA.
[Mikhailov, E. E.; Rew, H.; Romanov, G.; Zhang, M.] Coll William & Mary, Williamsburg, VA 23187 USA.
[Mirshekari, S.; Sturani, R.] Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, Brazil.
[Moore, C. J.] Univ Cambridge, Cambridge CB2 1TN, England.
[Nayak, R. K.; Samajdar, A.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[O'Dell, J.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England.
[Ogin, G. H.] Whitman Coll, 345 Boyer Ave, Walla Walla, WA 99362 USA.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Daejeon 305390, South Korea.
[Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Rosinska, D.] Univ Zielona Gora, Janusz Gil Inst Astron, PL-65265 Zielona Gora, Poland.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Trozzo, L.] Univ Siena, Via Laterina 8, I-53100 Siena, Italy.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Wade, L. E.; Wade, M.] Kenyon Coll, Gambier, OH 43022 USA.
[Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
RP Willis, JL (reprint author), Abilene Christian Univ, Abilene, TX 79699 USA.
EM lsc-spokesperson@ligo.org
RI Zhu, Xingjiang/E-1501-2016; Cesarini, Elisabetta/C-4507-2017;
Steinlechner, Sebastian/D-5781-2013; Chow, Jong/A-3183-2008; Frey,
Raymond/E-2830-2016; Prokhorov, Leonid/I-2953-2012; Ciani,
Giacomo/G-1036-2011; Di Virgilio, Angela Dora Vittoria/E-9078-2015;
Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Gammaitoni,
Luca/B-5375-2009; Ferrante, Isidoro/F-1017-2012; Chen,
Yanbei/A-2604-2013; Sorrentino, Fiodor/M-6662-2016; Garufi,
Fabio/K-3263-2015; Strigin, Sergey/I-8337-2012; McClelland,
David/E-6765-2010; Losurdo, Giovanni/K-1241-2014; Bondu,
Francois/A-2071-2012; Travasso, Flavio/J-9595-2016; Tiwari,
Shubhanshu/R-8546-2016; Bartos, Imre/A-2592-2017; Punturo,
Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Frasconi,
Franco/K-1068-2016; Vicere, Andrea/J-1742-2012; Sigg,
Daniel/I-4308-2015; Groot, Paul/K-4391-2016; Kumar, Prem/B-6691-2009;
Lazzaro, Claudia/L-2986-2016; Stratta, Maria Giuliana/L-3045-2016; De
Laurentis, Martina/L-3022-2016; Pinto, Innocenzo/L-3520-2016; Conti,
Livia/F-8565-2013; Vecchio, Alberto/F-8310-2015; Graef,
Christian/J-3167-2015; Branchesi, Marica/P-2296-2015; Nelemans,
Gijs/D-3177-2012; Piccinni, Ornella Juliana/C-1319-2016; Rocchi,
Alessio/O-9499-2015; Danilishin, Stefan/K-7262-2012; Tacca,
Matteo/J-1599-2015; Costa, Cesar/G-7588-2012; Gemme,
Gianluca/C-7233-2008; Puppo, Paola/J-4250-2012; Iyer, Bala
R./E-2894-2012; Leonardi, Matteo/G-9694-2015; Strain,
Kenneth/D-5236-2011; Marchesoni, Fabio/A-1920-2008; prodi,
giovanni/B-4398-2010;
OI Kanner, Jonah/0000-0001-8115-0577; Boer, Michel/0000-0001-9157-4349;
Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard
F/0000-0002-8501-8669; Murphy, David/0000-0002-8538-815X; Wang,
Gang/0000-0002-9668-8772; Pitkin, Matthew/0000-0003-4548-526X; Veitch,
John/0000-0002-6508-0713; Zhu, Xingjiang/0000-0001-7049-6468; Boschi,
Valerio/0000-0001-8665-2293; Papa, M.Alessandra/0000-0002-1007-5298;
Vocca, Helios/0000-0002-1200-3917; Farr, Ben/0000-0002-2916-9200; Guidi,
Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431;
Collette, Christophe/0000-0002-4430-3703; Addesso,
Paolo/0000-0003-0895-184X; Naticchioni, Luca/0000-0003-2918-0730; Khan,
Sebastian/0000-0003-4953-5754; Scott, Jamie/0000-0001-6701-6515;
Callister, Thomas/0000-0001-9892-177X; Sorazu,
Borja/0000-0002-6178-3198; Zweizig, John/0000-0002-1521-3397; Del Pozzo,
Walter/0000-0003-3978-2030; Cesarini, Elisabetta/0000-0001-9127-3167;
Steinlechner, Sebastian/0000-0003-4710-8548; Chow,
Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani,
Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora
Vittoria/0000-0002-2237-7533; Dolique, Vincent/0000-0001-5644-9905;
O'Shaughnessy, Richard/0000-0001-5832-8517; Gammaitoni,
Luca/0000-0002-4972-7062; Ferrante, Isidoro/0000-0002-0083-7228;
Sorrentino, Fiodor/0000-0002-9605-9829; Garufi,
Fabio/0000-0003-1391-6168; McClelland, David/0000-0001-6210-5842;
Losurdo, Giovanni/0000-0003-0452-746X; Bondu,
Francois/0000-0001-6487-5197; Travasso, Flavio/0000-0002-4653-6156;
Tiwari, Shubhanshu/0000-0003-1611-6625; Punturo,
Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338;
Frasconi, Franco/0000-0003-4204-6587; Vicere,
Andrea/0000-0003-0624-6231; Sigg, Daniel/0000-0003-4606-6526; Groot,
Paul/0000-0002-4488-726X; Lazzaro, Claudia/0000-0001-5993-3372; Stratta,
Maria Giuliana/0000-0003-1055-7980; De Laurentis,
Martina/0000-0002-3815-4078; Conti, Livia/0000-0003-2731-2656; Vecchio,
Alberto/0000-0002-6254-1617; Graef, Christian/0000-0002-4535-2603;
Nelemans, Gijs/0000-0002-0752-2974; Piccinni, Ornella
Juliana/0000-0001-5478-3950; Rocchi, Alessio/0000-0002-1382-9016;
Danilishin, Stefan/0000-0001-7758-7493; Tacca,
Matteo/0000-0003-1353-0441; Gemme, Gianluca/0000-0002-1127-7406; Puppo,
Paola/0000-0003-4677-5015; Iyer, Bala R./0000-0002-4141-5179; Strain,
Kenneth/0000-0002-2066-5355; Marchesoni, Fabio/0000-0001-9240-6793;
prodi, giovanni/0000-0001-5256-915X; Gendre, Bruce/0000-0002-9077-2025;
Granata, Massimo/0000-0003-3275-1186; Berry,
Christopher/0000-0003-3870-7215; Davies, Gareth/0000-0002-4289-3439;
Principe, Maria/0000-0002-6327-0628
FU Australian Research Council; EGO consortium; Council of Scientific and
Industrial Research of India; Department of Science and Technology,
India; Science AMP; Engineering Research Board (SERB), India; Ministry
of Human Resource Development, India; Spanish Ministerio de Economia y
Competitividad; Conselleria d'Economia i Competitivitat; Conselleria
d'Educacio, Cultura i Universitats of the Govern de les Illes Balears;
National Science Centre of Poland; European Commission; Royal Society;
Scottish Funding Council; Scottish Universities Physics Alliance;
Hungarian Scientific Research Fund (OTKA); Lyon Institute of Origins
(LIO); National Research Foundation of Korea; Industry Canada; Province
of Ontario through the Ministry of Economic Development and Innovation;
Natural Science and Engineering Research Council Canada; Canadian
Institute for Advanced Research; Brazilian Ministry of Science,
Technology, and Innovation; Russian Foundation for Basic Research;
Leverhulme Trust; Research Corporation; Ministry of Science and
Technology (MOST), Taiwan; Kavli Foundation
FX The authors gratefully acknowledge the support of the United States
National Science Foundation (NSF) for the construction and operation of
the LIGO Laboratory and Advanced LIGO as well as the Science and
Technology Facilities Council (STFC) of the United Kingdom, the
Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for
support of the construction of Advanced LIGO and construction and
operation of the GEO600 detector. Additional support for Advanced LIGO
was provided by the Australian Research Council. The authors gratefully
acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN),
the French Centre National de la Recherche Scientifique (CNRS) and the
Foundation for Fundamental Research on Matter supported by the
Netherlands Organisation for Scientific Research, for the construction
and operation of the Virgo detector and the creation and support of the
EGO consortium. The authors also gratefully acknowledge research support
from these agencies as well as by the Council of Scientific and
Industrial Research of India, Department of Science and Technology,
India, Science & Engineering Research Board (SERB), India, Ministry of
Human Resource Development, India, the Spanish Ministerio de Economia y
Competitividad, the Conselleria d'Economia i Competitivitat and
Conselleria d'Educacio, Cultura i Universitats of the Govern de les
Illes Balears, the National Science Centre of Poland, the European
Commission, the Royal Society, the Scottish Funding Council, the
Scottish Universities Physics Alliance, the Hungarian Scientific
Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National
Research Foundation of Korea, Industry Canada and the Province of
Ontario through the Ministry of Economic Development and Innovation, the
Natural Science and Engineering Research Council Canada, Canadian
Institute for Advanced Research, the Brazilian Ministry of Science,
Technology, and Innovation, Russian Foundation for Basic Research, the
Leverhulme Trust, the Research Corporation, Ministry of Science and
Technology (MOST), Taiwan and the Kavli Foundation. The authors
gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and
the State of Niedersachsen/Germany for provision of computational
resources.
NR 54
TC 39
Z9 39
U1 18
U2 48
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD MAR 31
PY 2016
VL 116
IS 13
AR 131102
DI 10.1103/PhysRevLett.116.131102
PG 12
WC Physics, Multidisciplinary
SC Physics
GA DH9EQ
UT WOS:000373099600001
ER
PT J
AU Fujita, S
Kataoka, R
Fujii, I
Pulkkinen, A
Watari, S
AF Fujita, Shigeru
Kataoka, Ryuho
Fujii, Ikuko
Pulkkinen, Antti
Watari, Shinichi
TI Extremely severe space weather and geomagnetically induced currents in
regions with locally heterogeneous ground resistivity
SO EARTH PLANETS AND SPACE
LA English
DT Editorial Material
ID SOLAR-TYPE STARS; AURORAL ELECTROJET; FIELD OBSERVATIONS; MAGNETIC
STORMS; POWER NETWORK; SYSTEM; CONDUCTIVITY; DISTRIBUTIONS; SUPERFLARES;
SIMULATION
C1 [Fujita, Shigeru; Fujii, Ikuko] Meteorol Coll, Kashiwa, Chiba, Japan.
[Kataoka, Ryuho] Natl Inst Polar Res, Tachikawa, Tokyo, Japan.
[Pulkkinen, Antti] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Watari, Shinichi] Natl Inst Informat & Communicat Technol, Koganei, Tokyo, Japan.
RP Fujita, S (reprint author), Meteorol Coll, Kashiwa, Chiba, Japan.
EM sfujita@mc-jma.go.jp
NR 24
TC 1
Z9 1
U1 2
U2 5
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1880-5981
J9 EARTH PLANETS SPACE
JI Earth Planets Space
PD MAR 31
PY 2016
VL 68
AR 51
DI 10.1186/s40623-016-0428-y
PG 3
WC Geosciences, Multidisciplinary
SC Geology
GA DI1KZ
UT WOS:000373256300001
ER
PT J
AU Terada, M
Seki, M
Takahashi, R
Yamada, S
Higashibata, A
Majima, HJ
Sudoh, M
Mukai, C
Ishioka, N
AF Terada, Masahiro
Seki, Masaya
Takahashi, Rika
Yamada, Shin
Higashibata, Akira
Majima, Hideyuki J.
Sudoh, Masamichi
Mukai, Chiaki
Ishioka, Noriaki
TI Effects of a Closed Space Environment on Gene Expression in Hair
Follicles of Astronauts in the International Space Station
SO PLOS ONE
LA English
DT Article
ID CELLS; STEM; SPACEFLIGHT; MERCURY; RNA; MICROGRAVITY; POLLUTION;
INCREASES; JAPANESE; INDUCE
AB Adaptation to the space environment can sometimes pose physiological problems to International Space Station (ISS) astronauts after their return to earth. Therefore, it is important to develop healthcare technologies for astronauts. In this study, we examined the feasibility of using hair follicles, a readily obtained sample, to assess gene expression changes in response to spaceflight adaptation. In order to investigate the gene expression changes in human hair follicles during spaceflight, hair follicles of 10 astronauts were analyzed by microarray and real time qPCR analyses. We found that spaceflight alters human hair follicle gene expression. The degree of changes in gene expression was found to vary among individuals. In some astronauts, genes related to hair growth such as FGF18, ANGPTL7 and COMP were upregulated during flight, suggesting that spaceflight inhibits cell proliferation in hair follicles.
C1 [Terada, Masahiro; Sudoh, Masamichi] Jikei Univ, Sch Med, Div Aerosp Med, Minato Ku, Tokyo, Japan.
[Terada, Masahiro; Yamada, Shin; Higashibata, Akira; Sudoh, Masamichi; Mukai, Chiaki; Ishioka, Noriaki] Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki, Japan.
[Terada, Masahiro] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
[Seki, Masaya; Takahashi, Rika] Adv Engn Serv Co Ltd, Tsukuba, Ibaraki, Japan.
[Higashibata, Akira; Majima, Hideyuki J.; Ishioka, Noriaki] Kagoshima Univ, Grad Sch Med & Dent Sci, Kagoshima, Kagoshima 890, Japan.
[Ishioka, Noriaki] Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229, Japan.
[Ishioka, Noriaki] SOKENDAI, Sch Phys Sci, Dept Space & Astronaut Sci, Sagamihara, Kanagawa, Japan.
RP Terada, M (reprint author), Jikei Univ, Sch Med, Div Aerosp Med, Minato Ku, Tokyo, Japan.; Terada, M (reprint author), Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki, Japan.; Terada, M (reprint author), NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
EM terada.masahiro@jikei.ac.jp
FU Japan Aerospace Exploration Agency (JAXA); Advanced Engineering Services
Co., Ltd.
FX The experimental cost for this study was funded by Japan Aerospace
Exploration Agency (JAXA). Advanced Engineering Services Co., Ltd.
provided support in the form of salaries for authors MS (2nd author) and
RT, but did not have any additional role in the study design, data
collection and analysis, decision to publish, or preparation of the
manuscript. The specific roles of these authors are articulated in the
'author contributions' section.
NR 51
TC 4
Z9 4
U1 1
U2 2
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD MAR 30
PY 2016
VL 11
IS 3
AR e0150801
DI 10.1371/journal.pone.0150801
PG 17
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DH9LB
UT WOS:000373116500009
PM 27029003
ER
PT J
AU Cudahy, T
Caccetta, M
Thomas, M
Hewson, R
Abrams, M
Kato, M
Kashimura, O
Ninomiya, Y
Yamaguchi, Y
Collings, S
Laukamp, C
Ong, C
Lau, I
Rodger, A
Chia, J
Warren, P
Woodcock, R
Fraser, R
Rankine, T
Vote, J
de Caritat, P
English, P
Meyer, D
Doescher, C
Fu, BH
Shi, PL
Mitchell, R
AF Cudahy, Thomas
Caccetta, Mike
Thomas, Matilda
Hewson, Robert
Abrams, Michael
Kato, Masatane
Kashimura, Osamu
Ninomiya, Yoshiki
Yamaguchi, Yasushi
Collings, Simon
Laukamp, Carsten
Ong, Cindy
Lau, Ian
Rodger, Andrew
Chia, Joanne
Warren, Peter
Woodcock, Robert
Fraser, Ryan
Rankine, Terry
Vote, Josh
de Caritat, Patrice
English, Pauline
Meyer, Dave
Doescher, Chris
Fu, Bihong
Shi, Pilong
Mitchell, Ross
TI Satellite-derived mineral mapping and monitoring of weathering,
deposition and erosion
SO SCIENTIFIC REPORTS
LA English
DT Article
ID CLAY-MINERALS; WESTERN-AUSTRALIA; SOIL PROPERTIES; CLIMATE-CHANGE;
DESERT DUST; OCEAN; TRANSPORT; IMAGERY; ASTER
AB The Earth's surface comprises minerals diagnostic of weathering, deposition and erosion. The first continental-scale mineral maps generated from an imaging satellite with spectral bands designed to measure clays, quartz and other minerals were released in 2012 for Australia. Here we show how these satellite mineral maps improve our understanding of weathering, erosional and depositional processes in the context of changing weather, climate and tectonics. The clay composition map shows how kaolinite has developed over tectonically stable continental crust in response to deep weathering during northwardly migrating tropical conditions from 45 to 10 Ma. The same clay composition map, in combination with one sensitive to water content, enables the discrimination of illite from montmorillonite clays that typically develop in large depositional environments over thin (sinking) continental crust such as the Lake Eyre Basin. Cutting across these clay patterns are sandy deserts that developed <10 Ma and are well mapped using another satellite product sensitive to the particle size of silicate minerals. This product can also be used to measure temporal gains/losses of surface clay caused by periodic wind erosion (dust) and rainfall inundation (flood) events. The accuracy and information content of these satellite mineral maps are validated using published data.
C1 [Cudahy, Thomas; Caccetta, Mike; Hewson, Robert; Laukamp, Carsten; Ong, Cindy; Lau, Ian; Rodger, Andrew; Fraser, Ryan; Rankine, Terry; Vote, Josh] Australian Resources Res Ctr, CSIRO Mineral Resources, 26 Dick Perry Ave, Kensington, WA 6151, Australia.
[Thomas, Matilda; de Caritat, Patrice; English, Pauline] Geosci Australia, GPO Box 378, Canberra, ACT 2601, Australia.
[Hewson, Robert] Sch Math & Geospatial Sci, GPO Box 2476, Melbourne, Vic 3001, Australia.
[Abrams, Michael] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kato, Masatane; Kashimura, Osamu] Japan Space Syst, Minato Ku, 3-5-8 Shibakoen, Tokyo 1050011, Japan.
[Ninomiya, Yoshiki] Geol Survey Japan, Natl Inst Adv Ind Sci & Technol, Cent 7,1-1-1 Higashi, Tsukuba, Ibaraki 3058567, Japan.
[Yamaguchi, Yasushi] Nagoya Univ, Grad Sch Environm Studies, Dept Earth & Environm Sci, Chikusa Ku, D2-1 510 Furo Cho, Nagoya, Aichi 4648601, Japan.
[Collings, Simon; Chia, Joanne] CSIRO Data61, Leeuwin Ctr, Brockway Rd, Floreat Pk, WA 6014, Australia.
[Warren, Peter] CSIRO Mineral Resources, Life Sci Ctr, Riverside Corp Pk,11 Julius Ave, N Ryde, NSW 2113, Australia.
[Woodcock, Robert] CSIRO Mineral Resources, Comp Sci & IT Bldg,108 North Rd, Canberra, ACT 2601, Australia.
[de Caritat, Patrice] Australian Natl Univ, Res Sch Earth Sci, GPO Box 4, Canberra, ACT 2601, Australia.
[Meyer, Dave; Doescher, Chris] USGS EROS, 47914 252nd Ave, Sioux Falls, SD 57198 USA.
[Fu, Bihong; Shi, Pilong] Chinese Acad Sci, Inst Remote Sensing & Digital Earth, 9 Dengzhuang South Rd, Beijing 100094, Peoples R China.
[Mitchell, Ross] CSIRO Oceans & Atmosphere, Forestry House,Banks Rd, Yarralumla, ACT 2601, Australia.
RP Cudahy, T (reprint author), Australian Resources Res Ctr, CSIRO Mineral Resources, 26 Dick Perry Ave, Kensington, WA 6151, Australia.
EM Thomas.Cudahy@csiro.au
OI de Caritat, Patrice/0000-0002-4185-9124
FU CSIRO; Geoscience Australia; ASTER Science Team; Japan Space Systems;
NASA-JPL; USGS; Chinese Academy of Sciences Remote Sensing and Digital
Earth; State and Territory geological surveys across Australia; Auscope
Grid; iVEC; NCI; Western Australian government's Centre of Excellence
for 3D Mineral Mapping (C3DMM)
FX This project was supported by CSIRO, Geoscience Australia, ASTER Science
Team, Japan Space Systems, NASA-JPL, USGS, Chinese Academy of Sciences
Remote Sensing and Digital Earth, State and Territory geological surveys
across Australia, Auscope Grid, iVEC, NCI and the Western Australian
government's Centre of Excellence for 3D Mineral Mapping (C3DMM). Work
by Mike Abrams was performed at the Jet Propulsion Lab/California
Institute of Technology under contract to the National Aeronautics and
Space Administration. Matilda Thomas, Patrice de Caritat and Pauline
English publish with permission from the Chief Executive Officer,
Geoscience Australia.
NR 62
TC 0
Z9 0
U1 3
U2 13
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD MAR 30
PY 2016
VL 6
AR 23702
DI 10.1038/srep23702
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DH8MK
UT WOS:000373047100001
PM 27025192
ER
PT J
AU Hesse, M
Liu, YH
Chen, LJ
Bessho, N
Kuznetsova, M
Birn, J
Burch, JL
AF Hesse, Michael
Liu, Yi-Hsin
Chen, Li-Jen
Bessho, Naoki
Kuznetsova, Masha
Birn, Joachim
Burch, James L.
TI On the electron diffusion region in asymmetric reconnection with a guide
magnetic field
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE magnetic reconnection; magnetopause; magnetospheric multiscale; kinetic
physics; distribution function; plasma physics
AB Particle-in-cell simulations in a 2.5-D geometry and analytical theory are employed to study the electron diffusion region in asymmetric reconnection with a guide magnetic field. The analysis presented here demonstrates that similar to the case without guide field, in-plane flow stagnation and null of the in-plane magnetic field are well separated. In addition, it is shown that the electric field at the local magnetic X point is again dominated by inertial effects, whereas it remains dominated by nongyrotropic pressure effects at the in-plane flow stagnation point. A comparison between local electron Larmor radii and the magnetic gradient scale lengths predicts that distribution should become nongyrotropic in a region enveloping both field reversal and flow stagnation points. This prediction is verified by an analysis of modeled electron distributions, which show clear evidence of mixing in the critical region.
C1 [Hesse, Michael; Liu, Yi-Hsin; Chen, Li-Jen; Bessho, Naoki; Kuznetsova, Masha] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.
[Birn, Joachim] Space Sci Inst, Boulder, CO USA.
[Birn, Joachim] Los Alamos Natl Lab, Los Alamos, NM USA.
[Burch, James L.] SW Res Inst, San Antonio, TX USA.
RP Hesse, M (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.
EM michael.hesse@nasa.gov
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NASA's Magnetospheric Multiscale mission; NSF [AGS-1543598, AGS-1552142]
FX This work was supported by NASA's Magnetospheric Multiscale mission and
NSF grants AGS-1543598 and AGS-1552142. Access to simulation data can be
provided upon request.
NR 15
TC 5
Z9 5
U1 2
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2016
VL 43
IS 6
BP 2359
EP 2364
DI 10.1002/2016GL068373
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA DK1TM
UT WOS:000374697200003
ER
PT J
AU Le, G
Luhr, H
Anderson, BJ
Strangeway, RJ
Russell, CT
Singer, H
Slavin, JA
Zhang, Y
Huang, T
Bromund, K
Chi, PJ
Lu, G
Fischer, D
Kepko, EL
Leinweber, HK
Magnes, W
Nakamura, R
Plaschke, F
Park, J
Rauberg, J
Stolle, C
Torbert, RB
AF Le, G.
Luehr, H.
Anderson, B. J.
Strangeway, R. J.
Russell, C. T.
Singer, H.
Slavin, J. A.
Zhang, Y.
Huang, T.
Bromund, K.
Chi, P. J.
Lu, G.
Fischer, D.
Kepko, E. L.
Leinweber, H. K.
Magnes, W.
Nakamura, R.
Plaschke, F.
Park, J.
Rauberg, J.
Stolle, C.
Torbert, R. B.
TI Magnetopause erosion during the 17 March 2015 magnetic storm: Combined
field-aligned currents, auroral oval, and magnetopause observations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE magnetopause erosion; magnetic reconnection; field-aligned currents;
Birkland currents; auroral oval; solar wind-magnetosphere interaction
ID SOLAR-WIND CONTROL; DAYSIDE MAGNETOSPHERE; BIRKELAND CURRENTS;
MAGNETOMETER DATA; FLUX TRANSFER; SHAPE; LOCATION; SYSTEM; MOTION; ANGLE
AB We present multimission observations of field-aligned currents, auroral oval, and magnetopause crossings during the 17 March 2015 magnetic storm. Dayside reconnection is expected to transport magnetic flux, strengthen field-aligned currents, lead to polar cap expansion and magnetopause erosion. Our multimission observations assemble evidence for all these manifestations. After a prolonged period of strongly southward interplanetary magnetic field, Swarm and AMPERE observe significant intensification of field-aligned currents. The dayside auroral oval, as seen by DMSP, appears as a thin arc associated with ongoing dayside reconnection. Both the field-aligned currents and the auroral arc move equatorward reaching as low as similar to 60 degrees magnetic latitude. Strong magnetopause erosion is evident in the in situ measurements of the magnetopause crossings by GOES 13/15 and MMS. The coordinated Swarm, AMPERE, DMSP, MMS and GOES observations, with both global and in situ coverage of the key regions, provide a clear demonstration of the effects of dayside reconnection on the entire magnetosphere.
C1 [Le, G.; Bromund, K.; Kepko, E. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Luehr, H.; Huang, T.; Rauberg, J.; Stolle, C.] GFZ German Res Ctr Geosci, Potsdam, Germany.
[Anderson, B. J.; Zhang, Y.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Strangeway, R. J.; Russell, C. T.; Chi, P. J.; Leinweber, H. K.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys & Earth, Los Angeles, CA USA.
[Strangeway, R. J.; Russell, C. T.; Chi, P. J.; Leinweber, H. K.] Univ Calif Los Angeles, Dept Space Sci, Los Angeles, CA USA.
[Singer, H.] NOAA, Space Weather Predict Ctr, Boulder, CO USA.
[Slavin, J. A.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Lu, G.] UCAR, High Altitude Observ, Boulder, CO USA.
[Fischer, D.; Magnes, W.; Nakamura, R.; Plaschke, F.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
[Park, J.] Korea Astron & Space Sci Inst, Daejeon, South Korea.
[Torbert, R. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
RP Le, G (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Guan.Le@nasa.gov
RI Nakamura, Rumi/I-7712-2013; Le, Guan/C-9524-2012; NASA MMS, Science
Team/J-5393-2013; Slavin, James/H-3170-2012; Zhang,
Yongliang/C-2180-2016
OI Nakamura, Rumi/0000-0002-2620-9211; Le, Guan/0000-0002-9504-5214; NASA
MMS, Science Team/0000-0002-9504-5214; Slavin,
James/0000-0002-9206-724X; Zhang, Yongliang/0000-0003-4851-1662
FU NSF [ATM-0739864, ATM-1420184]
FX We thank O. Le Contel and S. Petrinec for useful discussions. AMPERE
development, data acquisition, and science processing were supported by
NSF awards ATM-0739864 and ATM-1420184 to JHU/APL, and all products used
here are available via http://ampere.jhuapl.edu. We thank the JHU/APL
SSUSI team for providing the DMSP F18 SSUSI auroral data. The European
Space Agency is acknowledged for providing the Swarm data. The Swarm
data used in this paper are freely accessible at
https://earth.esa.int/guest/swarm/data-access. We acknowledge use of
NASA/GSFC's Space Physics Data Facility's CDAWeb service for obtaining
the ACE interplanetary magnetic field data, ACE solar wind plasma data,
and the SYM-H index. We acknowledge use of NOAA Space Weather Prediction
Center for obtaining GOES magnetometer data. We thank the entire team of
NASA's MMS mission for the dedication and expertise in its successful
development and operations.
NR 41
TC 3
Z9 3
U1 4
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2016
VL 43
IS 6
BP 2396
EP 2404
DI 10.1002/2016GL068257
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DK1TM
UT WOS:000374697200008
ER
PT J
AU Chen, LJ
Hesse, M
Wang, S
Bessho, N
Daughton, W
AF Chen, Li-Jen
Hesse, Michael
Wang, Shan
Bessho, Naoki
Daughton, William
TI Electron energization and structure of the diffusion region during
asymmetric reconnection
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE magnetic reconnection; electron diffusion region; electron acceleration;
electron heating; collisionless resistivity; collisionless dissipation
ID MAGNETIC RECONNECTION; X-LINE; PHYSICS
AB Results from particle-in-cell simulations of reconnection with asymmetric upstream conditions are reported to elucidate electron energization and structure of the electron diffusion region (EDR). Acceleration of unmagnetized electrons results in discrete structures in the distribution functions and supports the intense current and perpendicular heating in the EDR. The accelerated electrons are cyclotron turned by the reconnected magnetic field to produce the outflow jets, and as such, the acceleration by the reconnection electric field is limited, leading to resistivity without particle-particle or particle-wave collisions. A map of electron distributions is constructed, and its spatial evolution is compared with quantities previously proposed to be EDR identifiers to enable effective identifications of the EDR in terrestrial magnetopause reconnection.
C1 [Chen, Li-Jen; Hesse, Michael; Wang, Shan; Bessho, Naoki] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Chen, Li-Jen; Wang, Shan; Bessho, Naoki] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Daughton, William] Los Alamos Natl Lab, Los Alamos, NM USA.
RP Chen, LJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.; Chen, LJ (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM li-jen.chen@nasa.gov
RI Daughton, William/L-9661-2013; NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NSF [AGS-1202537, AGS-1543598, AGS-1552142]; Theory and Modeling
Program; Fast Plasma Investigation of the Magnetospheric Multiscale
mission; NASA Heliophysics Theory Program
FX The research was supported in part by NSF grants AGS-1202537,
AGS-1543598, and AGS-1552142 and at NASA GSFC by the Theory and Modeling
Program and the Fast Plasma Investigation of the Magnetospheric
Multiscale mission. Contribution from W.D. was supported by NASA
Heliophysics Theory Program. The simulation runs were performed on
Pleiades under the NASA HEC Program and on Titan at the National Center
for Computational Sciences at ORNL. L.J.C. acknowledges the
contributions of J. Shuster and M. Argall to the PIC data plotting
software. The data are available upon request to the authors.
NR 28
TC 15
Z9 15
U1 4
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2016
VL 43
IS 6
BP 2405
EP 2412
DI 10.1002/2016GL068243
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DK1TM
UT WOS:000374697200009
ER
PT J
AU Morlighem, M
Bondzio, J
Seroussi, H
Rignot, E
Larour, E
Humbert, A
Rebuffi, S
AF Morlighem, M.
Bondzio, J.
Seroussi, H.
Rignot, E.
Larour, E.
Humbert, A.
Rebuffi, S.
TI Modeling of Store Gletscher's calving dynamics, West Greenland, in
response to ocean thermal forcing
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE glaciology; calving; ice-ocean interactions; Store Gletscher; inverse
modeling
ID OUTLET GLACIERS; ICE DYNAMICS; CLIMATE; RETREAT; FRONTS; SHEET; FLOW
AB Glacier-front dynamics is an important control on Greenland's ice mass balance. Warmer ocean waters trigger ice-front retreats of marine-terminating glaciers, and the corresponding loss in resistive stress leads to glacier acceleration and thinning. Here we present an approach to quantify the sensitivity and vulnerability of marine-terminating glaciers to ocean-induced melt. We develop a plan view model of Store Gletscher that includes a level set-based moving boundary capability, a parameterized ocean-induced melt, and a calving law with complete and precise land and fjord topographies to model the response of the glacier to increased melt. We find that the glacier is stabilized by a sill at its terminus. The glacier is dislodged from the sill when ocean-induced melt quadruples, at which point the glacier retreats irreversibly for 27km into a reverse bed. The model suggests that ice-ocean interactions are the triggering mechanism of glacier retreat, but the bed controls its magnitude.
C1 [Morlighem, M.; Bondzio, J.; Rignot, E.; Rebuffi, S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Bondzio, J.; Humbert, A.] Helmholtz Ctr Polar & Marine Res, Alfred Wegener Inst, Bremerhaven, Germany.
[Seroussi, H.; Rignot, E.; Larour, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Morlighem, M (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
EM Mathieu.Morlighem@uci.edu
RI Rignot, Eric/A-4560-2014
OI Rignot, Eric/0000-0002-3366-0481
FU National Aeronautics and Space Administration, Cryospheric Sciences
Program [NNX15AD55G]
FX This work was performed at the Department of Earth System Science,
University of California, Irvine, under a contract with the National
Aeronautics and Space Administration, Cryospheric Sciences Program,
grant NNX15AD55G.
NR 34
TC 4
Z9 4
U1 8
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2016
VL 43
IS 6
BP 2659
EP 2666
DI 10.1002/2016GL067695
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DK1TM
UT WOS:000374697200040
ER
PT J
AU Rignot, E
Fenty, I
Xu, Y
Cai, C
Velicogna, I
Cofaigh, CO
Dowdeswell, JA
Weinrebe, W
Catania, G
Duncan, D
AF Rignot, E.
Fenty, I.
Xu, Y.
Cai, C.
Velicogna, I.
Cofaigh, C. O.
Dowdeswell, J. A.
Weinrebe, W.
Catania, G.
Duncan, D.
TI Bathymetry data reveal glaciers vulnerable to ice-ocean interaction in
Uummannaq and Vaigat glacial fjords, west Greenland
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID EAST GREENLAND; OUTLET GLACIERS; WATERS; SHELF; ACCELERATION;
VARIABILITY; RETREAT; ISBRAE; SHEET
AB Marine-terminating glaciers play a critical role in controlling Greenland's ice sheet mass balance. Their frontal margins interact vigorously with the ocean, but our understanding of this interaction is limited, in part, by a lack of bathymetry data. Here we present a multibeam echo sounding survey of 14 glacial fjords in the Uummannaq and Vaigat fjords, west Greenland, which extends from the continental shelf to the glacier fronts. The data reveal valleys with shallow sills, overdeepenings (> 1300 m) from glacial erosion, and seafloor depths 100-1000 m deeper than in existing charts. Where fjords are deep enough, we detect the pervasive presence of warm, salty Atlantic Water (AW) (> 2.5 degrees C) with high melt potential, but we also find numerous glaciers grounded on shallow (< 200 m) sills, standing in cold (< 1 degrees C) waters in otherwise deep fjords, i.e., with reduced melt potential. Bathymetric observations extending to the glacier fronts are critical to understand the glacier evolution.
C1 [Rignot, E.; Xu, Y.; Cai, C.; Velicogna, I.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Rignot, E.; Fenty, I.; Velicogna, I.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Cofaigh, C. O.] Durahm Univ, Dept Geog, Durham, England.
[Dowdeswell, J. A.] Univ Cambridge, Scott Polar Res Inst, Cambridge CB2 1ER, England.
[Weinrebe, W.] GEOMAR Helmholtz Ctr Ocean Res, Kiel, Germany.
[Catania, G.; Duncan, D.] Univ Texas Austin, Inst Geophys, Austin, TX USA.
[Catania, G.; Duncan, D.] Univ Texas Austin, Dept Geol, Austin, TX 78712 USA.
RP Rignot, E (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.; Rignot, E (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM erignot@uci.edu
RI Rignot, Eric/A-4560-2014; Catania, Ginny/B-9787-2008
OI Rignot, Eric/0000-0002-3366-0481;
FU Gordon and Betty Moore Foundation [3280]; UC Irvine; NASA [NNX12AB86G,
NNX12AP50G]; Jackson School of Geosciences; UK Natural Environment
Research Council [NE/D001986/1]; UK NERC [NE/D001951/1]
FX This work was performed at the University of California Irvine under
grant 3280 from theGordon and Betty Moore Foundation, funds from UC
Irvine, and NASA grant NNX12AB86G; at Caltech's Jet Propulsion
Laboratory, Pasadena under a contract with NASA; funds from the Jackson
School of Geosciences and NASA grant NNX12AP50G for G.C.; and UK Natural
Environment Research Council Grant NE/D001986/1 for J.A.D. Collection of
the James Clark Ross multibeam data was funded by UK NERC grant
NE/D001951/1. We thank Captain Milos Simovic of Cape Race and his crew
for the 2013-2104 cruises and Captain Thorvald Jensen of the Esle and
his crew for the 2012 cruise. A 100m geotiff file is available at
ess.uci.edu/group/erignot/node/1535.
NR 30
TC 5
Z9 5
U1 6
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2016
VL 43
IS 6
BP 2667
EP 2674
DI 10.1002/2016GL067832
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DK1TM
UT WOS:000374697200041
ER
PT J
AU Palter, JB
Caron, CA
Law, KL
Willis, JK
Trossman, DS
Yashayaev, IM
Gilbert, D
AF Palter, Jaime B.
Caron, Charles-Andre
Law, Kara Lavender
Willis, Joshua K.
Trossman, David S.
Yashayaev, Igor M.
Gilbert, Denis
TI Variability of the directly observed, middepth subpolar North Atlantic
circulation
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MERIDIONAL OVERTURNING CIRCULATION; MID-DEPTH CIRCULATION; INTERANNUAL
VARIABILITY; SEA-WATER; PATHWAYS; LABRADOR; OCEAN; CURRENTS; WESTERN;
IMPACT
AB Satellite views of the ocean have suggested a decline of the subpolar North Atlantic surface circulation during the 1990s and 2000s. This was a period of unprecedented observational capacity in the basin, thanks to the presence of many hundreds of profiling floats. We use more than 40,000 subsurface displacements of these floats to characterize the circulation at 1000m depth, and its evolution from 1997-2013. We show a statistically significant slowdown in the Labrador Sea boundary currents of -0.8 cm s(-1) per decade (95% confidence interval of -1.4 to -0.15 cm s(-1) per decade, a conservative estimate of the uncertainty). Otherwise, the middepth circulation field was largely stable. Our analysis of the location where the North Atlantic Current crosses the Mid-Atlantic Ridge shows that profiling floats can reveal steering by bathymetric features, but do not reveal of decadal variability in the position where the current crosses the ridge.
C1 [Palter, Jaime B.] Univ Rhode Isl, Grad Sch Oceanog, Kingston, RI 02881 USA.
[Palter, Jaime B.; Caron, Charles-Andre; Trossman, David S.] McGill Univ, Atmospher & Ocean Sci Dept, Montreal, PQ, Canada.
[Law, Kara Lavender] Sea Educ Assoc, Woods Hole, MA USA.
[Willis, Joshua K.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Trossman, David S.] Goddard Earth Sci Technol & Res, Greenbelt, MD USA.
[Trossman, David S.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Yashayaev, Igor M.] Fisheries & Oceans Canada, Bedford Inst Oceanog, POB 1006, Dartmouth, NS B2Y 4A2, Canada.
[Gilbert, Denis] Fisheries & Oceans Canada, Maurice Lamontagne Inst, Mont Joli, PQ G5H 3Z4, Canada.
RP Palter, JB (reprint author), Univ Rhode Isl, Grad Sch Oceanog, Kingston, RI 02881 USA.; Palter, JB (reprint author), McGill Univ, Atmospher & Ocean Sci Dept, Montreal, PQ, Canada.
EM jpalter@uri.edu
RI Gilbert, Denis/A-3067-2010
OI Gilbert, Denis/0000-0002-9554-9594
FU NSERC
FX We gratefully acknowledge the creators of the CARS ocean atlas
(http://www.marine.csiro.au/similar to dunn/cars2009/), the contributors
to the Andro (http://wwz.ifremer.fr/lpo/Produits/ANDRO) and YoMaHa
(http://apdrc.soest.hawaii.edu/projects/yomaha/) quality-controlled
float displacement databases, and the Aviso program
(http://www.aviso.altimetry.fr/en/data.html) for making the satellite
based dynamic topography available. Data from the early float
experiments are largely available at http://woce.nodc.noaa.gov/wdiu and
are available by request to J.B.P. We are also indebted to the many
scientists and crews who contribute to the success of the global Argo
program. This manuscript was improved by insightful reviews from Peter
Rhines and three anonymous reviewers. Funding for this work was provided
by NSERC's program on Climate Change and Atmospheric Research via the
Ventilations, Interactions and Transports Across the Labrador Sea
(VITALS) program. All 1000 m velocity maps are available by request to
J.B.P.
NR 27
TC 2
Z9 2
U1 2
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2016
VL 43
IS 6
BP 2700
EP 2708
DI 10.1002/2015GL067235
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DK1TM
UT WOS:000374697200045
ER
PT J
AU Samset, BH
Myhre, G
Forster, PM
Hodnebrog, O
Andrews, T
Faluvegi, G
Flaschner, D
Kasoar, M
Kharin, V
Kirkevag, A
Lamarque, JF
Olivie, D
Richardson, T
Shindell, D
Shine, KP
Takemura, T
Voulgarakis, A
AF Samset, B. H.
Myhre, G.
Forster, P. M.
Hodnebrog, O.
Andrews, T.
Faluvegi, G.
Flaeschner, D.
Kasoar, M.
Kharin, V.
Kirkevag, A.
Lamarque, J-F.
Olivie, D.
Richardson, T.
Shindell, D.
Shine, K. P.
Takemura, T.
Voulgarakis, A.
TI Fast and slow precipitation responses to individual climate forcers: A
PDRMIP multimodel study
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE precipitation; climate drivers; PDRMIP
ID BLACK CARBON; HYDROLOGIC-CYCLE; ALTITUDE; DIOXIDE; SPREAD
AB Precipitation is expected to respond differently to various drivers of anthropogenic climate change. We present the first results from the Precipitation Driver and Response Model Intercomparison Project (PDRMIP), where nine global climate models have perturbed CO2, CH4, black carbon, sulfate, and solar insolation. We divide the resulting changes to global mean and regional precipitation into fast responses that scale with changes in atmospheric absorption and slow responses scaling with surface temperature change. While the overall features are broadly similar between models, we find significant regional intermodel variability, especially over land. Black carbon stands out as a component that may cause significant model diversity in predicted precipitation change. Processes linked to atmospheric absorption are less consistently modeled than those linked to top-of-atmosphere radiative forcing. We identify a number of land regions where the model ensemble consistently predicts that fast precipitation responses to climate perturbations dominate over the slow, temperature-driven responses.
C1 [Samset, B. H.; Myhre, G.; Hodnebrog, O.] Ctr Int Climate & Environm Res, Oslo, Norway.
[Forster, P. M.; Richardson, T.] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England.
[Andrews, T.] Met Off Hadley Ctr, Exeter, Devon, England.
[Faluvegi, G.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Flaeschner, D.] Max Planck Inst Meteorol, Bundesstr 55, D-20146 Hamburg, Germany.
[Kasoar, M.; Voulgarakis, A.] Univ London Imperial Coll Sci Technol & Med, Fac Nat Sci, Dept Phys, London, England.
[Kharin, V.] Canadian Ctr Climate Modelling & Anal, Gatineau, PQ, Canada.
[Kirkevag, A.; Olivie, D.] Norwegian Meteorol Inst, Oslo, Norway.
[Lamarque, J-F.] UCAR, NCAR, Boulder, CO USA.
[Shindell, D.] Duke Univ, Nicholas Sch Environm, Durham, NC USA.
[Shine, K. P.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Takemura, T.] Kyushu Univ, Res Inst Appl Mech, Fukuoka 812, Japan.
RP Samset, BH (reprint author), Ctr Int Climate & Environm Res, Oslo, Norway.
EM b.h.samset@cicero.oslo.no
RI Shine, Keith/D-9093-2012; Takemura, Toshihiko/C-2822-2009; Kyushu,
RIAM/F-4018-2015; Myhre, Gunnar/A-3598-2008; Forster, Piers/F-9829-2010;
OI Shine, Keith/0000-0003-2672-9978; Takemura,
Toshihiko/0000-0002-2859-6067; Myhre, Gunnar/0000-0002-4309-476X;
Forster, Piers/0000-0002-6078-0171; Richardson,
Thomas/0000-0002-3947-9915
FU Research Council of Norway, through the grant NAPEX [229778]; Natural
Environment Research Council [NE/K500872/1]; supercomputer system of the
National Institute for Environmental Studies, Japan; Environment
Research and Technology Development Fund of the Ministry of the
Environment, Japan [S-12-3]; JSPS [15H01728, 15 K12190]; Norwegian
Research Council [229771, 207711/E10, nn2345k, ns2345k]; NERC
[NE/K007483/1]; National Science Foundation; Joint UK DECC/Defra Met
Office Hadley Centre Climate Programme [GA01101]
FX All model results used for the present study are available to the public
through the Norwegian NORSTORE data storage facility. B.H.S., G.M., and
O.H. were funded by the Research Council of Norway, through the grant
NAPEX (229778). Supercomputer facilities were generously provided by
NOTUR. D.S. thanks the NASA High-End Computing Program through the NASA
Center for Climate Simulation at Goddard Space Flight Center for
computational resources. M.K. and A.V. are supported by the Natural
Environment Research Council under grant NE/K500872/1. Simulations with
HadGEM3-GA4 were performed using the MONSooN system, a collaborative
facility supplied under the Joint Weather and Climate Research
Programme, which is a strategic partnership between the Met Office and
the Natural Environment Research Council. T.T. was supported by the
supercomputer system of the National Institute for Environmental
Studies, Japan, the Environment Research and Technology Development Fund
(S-12-3) of the Ministry of the Environment, Japan, and JSPS KAKENHI
grants 15H01728 and 15 K12190. D.J.L.O. and A.K. were supported by the
Norwegian Research Council through the projects EVA (grant 229771) and
EarthClim (207711/E10), NOTUR (nn2345k), and NorStore (ns2345k)
projects. T.R. was supported by NERC training award NE/K007483/1 and
acknowledges the use of the MONSooN system. Computing resources for
J.F.L. (ark:/85065/d7wd3xhc) were provided by the Climate Simulation
Laboratory at NCAR's Computational and Information Systems Laboratory,
sponsored by the National Science Foundation and other agencies.
Computing resources for the simulations with the MPI model were provided
by the German Climate Computing Center (DKRZ), Hamburg. TA was supported
by the Joint UK DECC/Defra Met Office Hadley Centre Climate Programme
(GA01101).
NR 30
TC 5
Z9 5
U1 4
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2016
VL 43
IS 6
BP 2782
EP 2791
DI 10.1002/2016GL068064
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA DK1TM
UT WOS:000374697200055
ER
PT J
AU Rollins, AW
Thornberry, TD
Gao, RS
Woods, S
Lawson, RP
Bui, TP
Jensen, EJ
Fahey, DW
AF Rollins, A. W.
Thornberry, T. D.
Gao, R. S.
Woods, S.
Lawson, R. P.
Bui, T. P.
Jensen, E. J.
Fahey, D. W.
TI Observational constraints on the efficiency of dehydration mechanisms in
the tropical tropopause layer
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE cirrus; dehydration; TTL; stratospheric water vapor
ID STRATOSPHERIC WATER-VAPOR; HOMOGENEOUS ICE NUCLEATION; CIRRUS CLOUDS;
SUBVISIBLE CIRRUS; CRYSTAL NUMBERS; TRANSPORT; IMPACT; PROBE
AB The efficiency of dehydration in the tropical tropopause layer (TTL) determines how closely water vapor will be reduced to the lowest saturation mixing ratio encountered along a trajectory to the stratosphere, thereby strongly influencing stratospheric humidity. The NASA Airborne Tropical Tropopause Experiment (ATTREX) provided an unprecedented number and quality of in situ observations to constrain the key mechanisms controlling this dehydration. Statistical analyses of the ATTREX data show that nucleation, growth, and sedimentation each result in TTL dehydration becoming increasingly inefficient at temperatures below 200K. Because of these inefficiencies, models that ignore these mechanisms likely underestimate water vapor at the stratospheric entry point by 10-20% at the lowest temperatures.
C1 [Rollins, A. W.; Thornberry, T. D.; Gao, R. S.; Fahey, D. W.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Rollins, A. W.; Thornberry, T. D.; Fahey, D. W.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Woods, S.; Lawson, R. P.] SPEC Inc, Boulder, CO USA.
[Bui, T. P.; Jensen, E. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Rollins, AW (reprint author), NOAA, Earth Syst Res Lab, Boulder, CO USA.; Rollins, AW (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
EM Andrew.Rollins@noaa.gov
RI Fahey, David/G-4499-2013; Manager, CSD Publications/B-2789-2015
OI Fahey, David/0000-0003-1720-0634;
FU NOAA Atmospheric Chemistry; Carbon Cycle; Climate Program; NASA Airborne
Tropical Tropopause Experiment; NASA Radiation Sciences Program
FX We thank the Armstrong Flight Research Center Global Hawk crew and
pilots for making these measurements possible. This research was funded
by the NOAA Atmospheric Chemistry, Carbon Cycle, and Climate Program,
the NASA Airborne Tropical Tropopause Experiment, and the NASA Radiation
Sciences Program. Data used in this analysis are archived by NASA
(https://espoarchive.nasa.gov/archive/browse/attrex).
NR 33
TC 2
Z9 2
U1 3
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2016
VL 43
IS 6
BP 2912
EP 2918
DI 10.1002/2016GL067972
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DK1TM
UT WOS:000374697200071
ER
PT J
AU Guan, B
Waliser, DE
Ralph, FM
Fetzer, EJ
Neiman, PJ
AF Guan, Bin
Waliser, Duane E.
Ralph, F. Martin
Fetzer, Eric J.
Neiman, Paul J.
TI Hydrometeorological characteristics of rain-on-snow events associated
with atmospheric rivers
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE atmospheric rivers; rain-on-snow; hydrometeorological characteristics
ID WESTERN UNITED-STATES; NORTHERN CALIFORNIA; SIERRA-NEVADA;
PRECIPITATION; VARIABILITY; SATELLITE; LANDFALLS; IMPACTS; SEASON; RADAR
AB Atmospheric rivers (ARs) are narrow, elongated, synoptic corridors of enhanced water vapor transport that play an important role in regional weather/hydrology. Rain-on-snow (ROS) events during ARs present enhanced flood risks due to the combined effects of rainfall and snowmelt. Focusing on California's Sierra Nevada, the study identifies ROS occurrences and their connection with ARs during the 1998-2014 winters. AR conditions, which occur during 17% of all precipitation events, are associated with 50% of ROS events (25 of 50). Composite analysis shows that compared to ARs without ROS, ARs with ROS are on average warmer by 2K, with snow water equivalent loss of 0.7cm/d (providing 20% of the combined water available for runoff) and 50% larger streamflow/precipitation ratios. Atmospheric Infrared Sounder retrievals reveal distinct offshore characteristics of the two types of ARs. The results highlight the potential value of observing these events for snow, rain, and flood prediction.
C1 [Guan, Bin; Waliser, Duane E.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Guan, Bin; Waliser, Duane E.; Fetzer, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Ralph, F. Martin] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Western Weather & Water Extremes, La Jolla, CA 92093 USA.
[Neiman, Paul J.] NOAA, Earth Syst Res Lab, Phys Sci Div, Boulder, CO USA.
RP Guan, B (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.; Guan, B (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM bin.guan@jpl.nasa.gov
RI Guan, Bin/F-6735-2010
FU NASA Energy and Water cycle Study (NEWS) program; California Department
of Water Resources
FX This research was supported by the NASA Energy and Water cycle Study
(NEWS) program and the California Department of Water Resources. D.E.
W.'s and E.J.F.'s contributions to this study were carried out on behalf
of the Jet Propulsion Laboratory, California Institute of Technology,
and F.M.R.'s at Scripps Institution of Oceanography, under a contract
with the National Aeronautics and Space Administration.
NR 28
TC 1
Z9 1
U1 7
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2016
VL 43
IS 6
BP 2964
EP 2973
DI 10.1002/2016GL067978
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA DK1TM
UT WOS:000374697200077
ER
PT J
AU Cantrell, JH
Cantrell, SA
AF Cantrell, John H.
Cantrell, Sean A.
TI Bifurcation, chaos, and scan instability in dynamic atomic force
microscopy
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID ACOUSTIC MICROSCOPY; INTERMITTENT-CONTACT; TIP; VIBRATIONS; POLYMER;
SURFACE; AFM
AB The dynamical motion at any point on the cantilever of an atomic force microscope can be expressed quite generally as a superposition of simple harmonic oscillators corresponding to the vibrational modes allowed by the cantilever shape. Central to the dynamical equations is the representation of the cantilever-sample interaction force as a polynomial expansion with coefficients that account for the interaction force "stiffness," the cantilever-to-sample energy transfer, and the displacement amplitude of cantilever oscillation. Renormalization of the cantilever beam model shows that for a given cantilever drive frequency cantilever dynamics can be accurately represented by a single nonlinear mass-spring model with frequency-dependent stiffness and damping coefficients [S. A. Cantrell and J. H. Cantrell, J. Appl. Phys. 110, 094314 (2011)]. Application of the Melnikov method to the renormalized dynamical equation is shown to predict a cascade of period doubling bifurcations with increasing cantilever drive force that terminates in chaos. The threshold value of the drive force necessary to initiate bifurcation is shown to depend strongly on the cantilever setpoint and drive frequency, effective damping coefficient, nonlinearity of the cantilever-sample interaction force, and the displacement amplitude of cantilever oscillation. The model predicts the experimentally observed interruptions of the bifurcation cascade for cantilevers of sufficiently large stiffness. Operational factors leading to the loss of image quality in dynamic atomic force microscopy are addressed, and guidelines for optimizing scan stability are proposed using a quantitative analysis based on system dynamical parameters and choice of feedback loop parameter. (C) 2016 AIP Publishing LLC.
C1 [Cantrell, John H.] NASA, Res Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
[Cantrell, Sean A.] NLS Analyt LLC, 375 Dundee Rd, Glencoe, IL 60022 USA.
RP Cantrell, JH (reprint author), NASA, Res Directorate, Langley Res Ctr, Hampton, VA 23681 USA.; Cantrell, SA (reprint author), NLS Analyt LLC, 375 Dundee Rd, Glencoe, IL 60022 USA.
EM john.h.cantrell@nasa.gov; scantrell@nlsanalytics.com
FU Materials Genome Project; Advanced Composite Program at NASA Langley
Research Center, Hampton, Virginia, USA
FX This work was supported by the Materials Genome Project and the Advanced
Composite Program at NASA Langley Research Center, Hampton, Virginia,
USA.
NR 41
TC 0
Z9 0
U1 10
U2 12
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-8979
EI 1089-7550
J9 J APPL PHYS
JI J. Appl. Phys.
PD MAR 28
PY 2016
VL 119
IS 12
AR 125308
DI 10.1063/1.4944714
PG 12
WC Physics, Applied
SC Physics
GA DI6II
UT WOS:000373602000063
ER
PT J
AU Xia, YL
Cosgrove, BA
Mitchell, KE
Peters-Lidard, CD
Ek, MB
Brewer, M
Mocko, D
Kumar, SV
Wei, HL
Meng, J
Luo, LF
AF Xia, Youlong
Cosgrove, Brian A.
Mitchell, Kenneth E.
Peters-Lidard, Christa D.
Ek, Michael B.
Brewer, Michael
Mocko, David
Kumar, Sujay V.
Wei, Helin
Meng, Jesse
Luo, Lifeng
TI Basin-scale assessment of the land surface water budget in the National
Centers for Environmental Prediction operational and research NLDAS-2
systems
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE NCEP operational NLDAS-2; USGS HUG8 runoff; gridded FLUXNET ET;
basin-scale assessment; water budget components; River Forecast Center
ID DATA ASSIMILATION SYSTEM; TIME-VARIABLE GRAVITY; MESOSCALE ETA-MODEL;
SOIL-MOISTURE; UNITED-STATES; BIOSPHERE MODEL; EVAPOTRANSPIRATION;
BALANCE; FLUXNET; TEMPERATURE
AB The purpose of this study is to evaluate the components of the land surface water budget in the four land surface models (Noah, SAC-Sacramento Soil Moisture Accounting Model, (VIC) Variable Infiltration Capacity Model, and Mosaic) applied in the newly implemented National Centers for Environmental Prediction (NCEP) operational and research versions of the North American Land Data Assimilation System version 2 (NLDAS-2). This work focuses on monthly and annual components of the water budget over 12 National Weather Service (NWS) River Forecast Centers (RFCs). Monthly gridded FLUX Network (FLUXNET) evapotranspiration (ET) from the Max-Planck Institute (MPI) of Germany, U.S. Geological Survey (USGS) total runoff (Q), changes in total water storage (dS/dt, derived as a residual by utilizing MPI ET and USGS Q in the water balance equation), and Gravity Recovery and Climate Experiment (GRACE) observed total water storage anomaly (TWSA) and change (TWSC) are used as reference data sets. Compared to these ET and Q benchmarks, Mosaic and SAC (Noah and VIC) in the operational NLDAS-2 overestimate (underestimate) mean annual reference ET and underestimate (overestimate) mean annual reference Q. The multimodel ensemble mean (MME) is closer to the mean annual reference ET and Q. An anomaly correlation (AC) analysis shows good AC values for simulated monthly mean Q and dS/dt but significantly smaller AC values for simulated ET. Upgraded versions of the models utilized in the research side of NLDAS-2 yield largely improved performance in the simulation of these mean annual and monthly water component diagnostics. These results demonstrate that the three intertwined efforts of improving (1) the scientific understanding of parameterization of land surface processes, (2) the spatial and temporal extent of systematic validation of land surface processes, and (3) the engineering-oriented aspects such as parameter calibration and optimization are key to substantially improving product quality in various land data assimilation systems.
C1 [Xia, Youlong; Ek, Michael B.; Wei, Helin; Meng, Jesse] Natl Ctr Environm Predict, Envronm Modeling Ctr, College Pk, MD USA.
[Xia, Youlong; Wei, Helin; Meng, Jesse] NCEP EMC, IM Syst Grp, College Pk, MD USA.
[Cosgrove, Brian A.] Natl Water Ctr, Natl Weather Serv, Silver Spring, MD USA.
[Mitchell, Kenneth E.] Prescient Weather Ltd, State Coll, PA USA.
[Peters-Lidard, Christa D.; Mocko, David; Kumar, Sujay V.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD USA.
[Brewer, Michael] NESDIS NOAA, Natl Ctr Environm Informat, Asheville, NC USA.
[Mocko, David; Kumar, Sujay V.] NASA GSFC, SAIC, Greenbelt, MD USA.
[Luo, Lifeng] Michigan State Univ, Dept Geog, E Lansing, MI USA.
RP Xia, YL (reprint author), Natl Ctr Environm Predict, Envronm Modeling Ctr, College Pk, MD USA.
EM youlong.xia@noaa.gov
RI Peters-Lidard, Christa/E-1429-2012
OI Peters-Lidard, Christa/0000-0003-1255-2876
FU NOAA Office of Global Programs Global Energy and Water Cycle Experiment
(GEWEX) Americas Prediction Project (GAPP); NASA; NOAA Climate Program
Office (CPO) Climate Prediction Program of the Americas (CPPA) and
Modeling Analysis, Predictions, and Projections (MAPP)
FX NLDAS-1 research activities have been supported by the NOAA Office of
Global Programs Global Energy and Water Cycle Experiment (GEWEX)
Americas Prediction Project (GAPP) and the NASA Terrestrial Hydrology
Program. NLDAS-2 research and operational transition activities have
been supported by the NOAA Climate Program Office (CPO) Climate
Prediction Program of the Americas (CPPA) and Modeling Analysis,
Predictions, and Projections (MAPP). We acknowledge Dr. David Wolock,
who helped us create the HUC8 index mask file for the NLDAS-2 grid. We
also acknowledge Fanglin Yang and Hong Guan from EMC and three anonymous
reviewers whose review and comments greatly improved the quality of the
manuscript. All data including NLDAS-2 products, USGS runoff,
GRACE-observed TWSA and TWSC, and gridded FLUXNET data can be freely
accessed via public websites as described in the text.
NR 80
TC 1
Z9 1
U1 5
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 27
PY 2016
VL 121
IS 6
BP 2750
EP 2779
DI 10.1002/2015JD023733
PG 30
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DK1YB
UT WOS:000374710300015
ER
PT J
AU Minschwaner, K
Su, H
Jiang, JH
AF Minschwaner, K.
Su, H.
Jiang, J. H.
TI The upward branch of the Brewer-Dobson circulation quantified by
tropical stratospheric water vapor and carbon monoxide measurements from
the Aura Microwave Limb Sounder
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE stratosphere
ID QUASI-BIENNIAL OSCILLATION; TROPOPAUSE TEMPERATURES;
SATELLITE-OBSERVATIONS; DOWNWARD CONTROL; TAPE-RECORDER; CIRRUS CLOUDS;
OZONE; REANALYSES; CYCLE; AIR
AB The vertical distributions of water vapor (H2O) and carbon monoxide (CO) in the tropical lower stratosphere are controlled largely by their mixing ratios near the tropopause and by ascending motions as part of the Brewer-Dobson circulation (BDC). The upward propagation of seasonal variations imprinted on H2O and CO vertical profiles, often referred to as the tropical tape recorder, can be used to derive the mean vertical velocity, (w) over bar*, in this region of the lower stratosphere where quasi-horizontal mixing is not strong enough to erase the seasonal tape recorder signals. We used Aura Microwave Limb Sounder observations of the tropical tape recorders from 2004 to 2014 to derive values of (w) over bar* at pressures between 90 and 16hPa (about 18 to 28km altitude). Mean vertical profiles of (w) over bar* are consistent with calculated velocities derived from net radiative heating rates based on observed temperature, humidity, cloud, and trace gas amounts. Temporal variations in (w) over bar* are dominated by a quasi-biennial oscillation (QBO) and seasonal cycles, with maximum upwelling coinciding with easterly phases of the QBO in zonal wind shear and during the November-December period of the seasonal cycle. Both the QBO and annual modes emphasize the importance of wave phenomena in modulating the strength of tropical upwelling in the BDC. Interannual anomalies in (w) over bar* are correlated with variations in the El Nino-Southern Oscillation (ENSO), with enhanced stratospheric upwelling during El Nino phases and reduced upwelling during La Nina. A small decreasing linear trend (similar to 6%/decade) in (w) over bar* is observed from 2005 to 2014, although confidence is low in identifying such a trend as part of a long-term change due to the influence of ENSO over this period.
C1 [Minschwaner, K.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
[Su, H.; Jiang, J. H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Minschwaner, K (reprint author), New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
EM krm@nmt.edu
FU NASA
FX MLS v3.3 data are available from the NASA Goddard Space Flight Center
Earth Sciences (GES) Data and Information Services Center. Zonal wind
data were provided by the Institute for Meteorology at Freie Universitat
Berlin from their Web site at
http://www.geo.fu-berlin.de/en/met/ag/strat/produkte/qbo/. MEI and
interpolated OLR data provided by the NOAA/OAR/ESRL PSD, Boulder,
Colorado, USA, from their Web site at http://www.esrl.noaa.gov/psd. We
thank T. Janice Shen for the assistance with the radiative transfer
calculations. This work is partly performed at the Jet Propulsion
Laboratory, California Institute of Technology sponsored by NASA. The
authors acknowledge funding support by the NASA ROSES AST and NEWS
programs, and we are grateful for the time and effort of three anonymous
referees, who provided exceptionally useful comments and suggestions for
this paper.
NR 86
TC 5
Z9 5
U1 3
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 27
PY 2016
VL 121
IS 6
BP 2790
EP 2804
DI 10.1002/2015JD023961
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DK1YB
UT WOS:000374710300017
ER
PT J
AU Duderstadt, KA
Dibb, JE
Schwadron, NA
Spence, HE
Solomon, SC
Yudin, VA
Jackman, CH
Randall, CE
AF Duderstadt, Katharine A.
Dibb, Jack E.
Schwadron, Nathan A.
Spence, Harlan E.
Solomon, Stanley C.
Yudin, Valery A.
Jackman, Charles H.
Randall, Cora E.
TI Nitrate ion spikes in ice cores not suitable as proxies for solar proton
events
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE solar proton event; nitrate; SPE; WACCM
ID ENERGETIC PARTICLE EVENTS; OCTOBER-NOVEMBER 2003; MIDDLE ATMOSPHERE; ODD
NITROGEN; POLAR ICE; CARRINGTON EVENT; AD 774-775; PRECIPITATION EVENTS;
SPECTRA; MODEL
AB Nitrate ion spikes in polar ice cores are contentiously used to estimate the intensity, frequency, and probability of historical solar proton events, quantities that are needed to prepare for potentially society-crippling space weather events. We use the Whole Atmosphere Community Climate Model to calculate how large an event would have to be to produce enough odd nitrogen throughout the atmosphere to be discernible as nitrate peaks at the Earth's surface. These hypothetically large events are compared with probability of occurrence estimates derived from measured events, sunspot records, and cosmogenic radionuclides archives. We conclude that the fluence and spectrum of solar proton events necessary to produce odd nitrogen enhancements equivalent to the spikes of nitrate ions in Greenland ice cores are unlikely to have occurred throughout the Holocene, confirming that nitrate ions in ice cores are not suitable proxies for historical individual solar proton events.
C1 [Duderstadt, Katharine A.; Dibb, Jack E.; Schwadron, Nathan A.; Spence, Harlan E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Solomon, Stanley C.; Yudin, Valery A.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Yudin, Valery A.] Univ Colorado, CIRES, Space Weather Predict Ctr, Boulder, CO 80309 USA.
[Jackman, Charles H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Randall, Cora E.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Randall, Cora E.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
RP Duderstadt, KA (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
EM duderstadtk@eos.sr.unh.edu
RI Solomon, Stanley/J-4847-2012; Jackman, Charles/D-4699-2012; Randall,
Cora/L-8760-2014
OI Solomon, Stanley/0000-0002-5291-3034; Randall, Cora/0000-0002-4313-4397
FU NSF [1135432]; National Science Foundation; Office of Science (BER) of
the U.S. Department of Energy; NASA [NNX14AH54G]
FX This work was supported by NSF grant 1135432 to the University of New
Hampshire. We would like to acknowledge high-performance computing
support from Yellowstone (ark:/85065/d7wd3xhc) provided by NCAR's
Computational and Information Systems Laboratory, sponsored by the
National Science Foundation. The CESM project is supported by the
National Science Foundation and the Office of Science (BER) of the U.S.
Department of Energy. We also acknowledge the support of NASA grant
NNX14AH54G to the University of Colorado. We thank Colin Joyce for
providing PREDDICS model results as well as Marco Calisto, Eugene
Rozanov, and Ilya Usoskin and for providing ion pair production rates
for the Carrington-like events. The model data used to produce the
analysis and figures for this study are available upon request from the
corresponding author. We thank the reviewers of the manuscript for their
valuable comments and suggestions.
NR 107
TC 7
Z9 7
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 27
PY 2016
VL 121
IS 6
BP 2994
EP 3016
DI 10.1002/2015JD023805
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DK1YB
UT WOS:000374710300029
ER
PT J
AU Mehrotra, P
Djomehri, J
Heistand, S
Hood, R
Jin, HQ
Lazanoff, A
Saini, S
Biswas, R
AF Mehrotra, Piyush
Djomehri, Jahed
Heistand, Steve
Hood, Robert
Jin, Haoqiang
Lazanoff, Arthur
Saini, Subhash
Biswas, Rupak
TI Performance evaluation of Amazon Elastic Compute Cloud for NASA
high-performance computing applications
SO CONCURRENCY AND COMPUTATION-PRACTICE & EXPERIENCE
LA English
DT Article
DE cloud environments; high-performance application performance;
communication overhead; virtualization overhead
AB Cloud computing environments are now widely available and are being increasingly utilized for technical computing. They are also being touted for high-performance computing (HPC) applications in science and engineering. For example, Amazon Elastic Compute Cloud (EC2) Services offers specialized Cluster Compute instance types to run HPC applications. In this paper, we compare the performance characteristics of two Amazon EC2 HPC instance types with that of National Aeronautics and Space Administration's (NASA) Pleiades supercomputer, an SGI (R) ICE cluster. For this study, we utilized the HPC Challenge kernels and the NAS Parallel Benchmarks along with four full-scale applications from the repertoire of codes that are being used by NASA scientists and engineers. We compare the total runtime of these codes for varying number of cores. We also break out the computation and communication times for a subset of these applications to explore the effect of interconnect differences on the two systems. In general, the single node performance of the two platforms is equivalent. However, for most of the codes when scaling to larger core counts, the performance of the EC2 HPC instances generally lags that of Pleiades because of worse network performance of the former. In addition to analyzing application performance, we also briefly touch upon the overhead due to virtualization and the usability of cloud environments such as Amazon EC2. Published 2013. This article is a U.S. Government work and is in the public domain in the U.S.A.
C1 [Mehrotra, Piyush; Djomehri, Jahed; Heistand, Steve; Hood, Robert; Jin, Haoqiang; Lazanoff, Arthur; Saini, Subhash; Biswas, Rupak] NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA.
RP Mehrotra, P (reprint author), NASA, Ames Res Ctr, NAS Div, Moffett Field, CA 94035 USA.
EM piyush.mehrotra@nasa.gov
FU NASA [NNA07CA29C]
FX Work performed by J. Djomehri, S. Heistand, R. Hood, and A. Lazanoff was
supported by NASA Contract No. NNA07CA29C while they were employees of
Computer Sciences Corporation.
NR 11
TC 1
Z9 1
U1 2
U2 12
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1532-0626
EI 1532-0634
J9 CONCURR COMP-PRACT E
JI Concurr. Comput.-Pract. Exp.
PD MAR 25
PY 2016
VL 28
IS 4
SI SI
BP 1041
EP 1055
DI 10.1002/cpe.3029
PG 15
WC Computer Science, Software Engineering; Computer Science, Theory &
Methods
SC Computer Science
GA DE5BR
UT WOS:000370646300006
ER
PT J
AU Richardson, DE
Marancik, KE
Guyon, JR
Lutcavage, ME
Galuardi, B
Lam, CH
Walsh, HJ
Wildes, S
Yates, DA
Hare, JA
AF Richardson, David E.
Marancik, Katrin E.
Guyon, Jeffrey R.
Lutcavage, Molly E.
Galuardi, Benjamin
Lam, Chi Hin
Walsh, Harvey J.
Wildes, Sharon
Yates, Douglas A.
Hare, Jonathan A.
TI Discovery of a spawning ground reveals diverse migration strategies in
Atlantic bluefin tuna (Thunnus thynnus)
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE ichthyoplankton; Scombridae; large pelagic fish; pop-up satellite
archival tag; population structure
ID GULF-OF-MEXICO; WESTERN ATLANTIC; NORTHWESTERN ATLANTIC;
POPULATION-STRUCTURE; DIVING BEHAVIOR; THERMAL BIOLOGY; PACIFIC-OCEAN;
LIFE-HISTORY; LARVAE; SATELLITE
AB Atlantic bluefin tuna are a symbol of both the conflict between preservationist and utilitarian views of top ocean predators, and the struggle to reach international consensus on the management of migratory species. Currently, Atlantic bluefin tuna are managed as an early-maturing eastern stock, which spawns in the Mediterranean Sea, and a late-maturing western stock, which spawns in the Gulf of Mexico. However, electronic tagging studies show that many bluefin tuna, assumed to be of a mature size, do not visit either spawning ground during the spawning season. Whether these fish are spawning in an alternate location, skip-spawning, or not spawning until an older age affects how vulnerable this species is to anthropogenic stressors including exploitation. We use larval collections to demonstrate a bluefin tuna spawning ground in the Slope Sea, between the Gulf Stream and northeast United States continental shelf. We contend that western Atlantic bluefin tuna have a differential spawning migration, with larger individuals spawning in the Gulf of Mexico, and smaller individuals spawning in the Slope Sea. The current life history model, which assumes only Gulf of Mexico spawning, overestimates age at maturity for the western stock. Furthermore, individual tuna occupy both the Slope Sea and Mediterranean Sea in separate years, contrary to the prevailing view that individuals exhibit complete spawning-site fidelity. Overall, this complexity of spawning migrations questions whether there is complete independence in the dynamics of eastern and western Atlantic bluefin tuna and leads to lower estimates of the vulnerability of this species to exploitation and other anthropogenic stressors.
C1 [Richardson, David E.; Walsh, Harvey J.; Hare, Jonathan A.] NOAA, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Narragansett, RI 02882 USA.
[Marancik, Katrin E.] NOAA, Integrated Stat, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Narragansett, RI 02882 USA.
[Guyon, Jeffrey R.; Wildes, Sharon; Yates, Douglas A.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA.
[Lutcavage, Molly E.; Lam, Chi Hin] Univ Massachusetts Boston, Sch Environm, Large Pelag Res Ctr, Gloucester, MA 01931 USA.
[Galuardi, Benjamin] Univ Massachusetts Dartmouth, Sch Marine Sci & Technol, Fairhaven, MA 02719 USA.
[Galuardi, Benjamin] NOAA, Greater Atlantic Reg Fisheries Off, Natl Marine Fisheries Serv, Gloucester, MA 01930 USA.
RP Richardson, DE (reprint author), NOAA, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Narragansett, RI 02882 USA.
EM David.Richardson@noaa.gov
FU Presidential Early Career Award for Scientists and Engineers stipend
FX We thank the Northeast Fisheries Science Center (NEFSC) Protected
Species Branch for allowing us to sample plankton on their surveys; E.
Broughton and the scientific parties and crews of the NOAA vessels for
implementing the sampling; and fishermen tagging partners E. Murray, A.
Mendillo, W. Chaprales, M. Genovese, E. Clark, E. Stewart, E. Jacquard,
J. Jacquard, and C. Jacquard. M. Konieczna and the ichthyoplankton team
at the Morski Instytut Rybacki in Poland initially identified the
formalin-preserved larvae, and the scientists of the Canadian Centre for
DNA Barcoding sequenced the ethanol-preserved larvae. The Southeast
Fisheries Science Center Pelagic Observer Program provided observer
data. The late Capt. F. Cyganowski and P. C. Wilson are acknowledged for
their contribution to this work. R. Cowen, G. Heinisch, J. Manderson,
and R. Bell reviewed drafts of this manuscript. Funding for this work
was provided by a Presidential Early Career Award for Scientists and
Engineers stipend. Ship time was supported by NOAA, the Bureau of Ocean
Energy Management, and the US Navy through interagency agreements for
Atlantic Marine Assessment Program for Protected Species (AMAPPS).
NR 57
TC 7
Z9 7
U1 16
U2 32
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD MAR 22
PY 2016
VL 113
IS 12
BP 3299
EP 3304
DI 10.1073/pnas.1525636113
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DH0QH
UT WOS:000372488200057
PM 26951668
ER
PT J
AU Gandhiraman, RP
Singh, E
Diaz-Cartagena, DC
Nordlund, D
Koehne, J
Meyyappan, M
AF Gandhiraman, Ram P.
Singh, Eric
Diaz-Cartagena, Diana C.
Nordlund, Dennis
Koehne, Jessica
Meyyappan, M.
TI Plasma jet printing for flexible substrates
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID CELLULOSE PAPER; CARBON; NANOPARTICLES; SPECTROSCOPY; ELECTRONICS;
FABRICATION; EXCITATION; ALCOHOLS; NEXAFS; ACIDS
AB Recent interest in flexible electronics and wearable devices has created a demand for fast and highly repeatable printing processes suitable for device manufacturing. Robust printing technology is critical for the integration of sensors and other devices on flexible substrates such as paper and textile. An atmospheric pressure plasma-based printing process has been developed to deposit different types of nanomaterials on flexible substrates. Multiwalled carbon nanotubes were deposited on paper to demonstrate site-selective deposition as well as direct printing without any type of patterning. Plasma-printed nanotubes were compared with non-plasma-printed samples under similar gas flow and other experimental conditions and found to be denser with higher conductivity. The utility of the nanotubes on the paper substrate as a biosensor and chemical sensor was demonstrated by the detection of dopamine, a neurotransmitter, and ammonia, respectively. (C) 2016 AIP Publishing LLC.
C1 [Gandhiraman, Ram P.; Singh, Eric; Diaz-Cartagena, Diana C.; Koehne, Jessica; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Nordlund, Dennis] SLAC Natl Accelerator Lab, Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA 94025 USA.
RP Gandhiraman, RP (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
RI Nordlund, Dennis/A-8902-2008;
OI Nordlund, Dennis/0000-0001-9524-6908; Singh, Eric/0000-0001-7344-4495
FU Center Innovation Fund; NASA [NNX12AK33A]
FX This work in part was supported by the Center Innovation Fund. E.S. is a
high school senior at William S. Hart High School, Santa Clarita, CA.
D.C.D.C. was a student intern from the University of Puerto Rico. The
work by R.P.G. was supported by NASA contract to USRA under Award No.
NNX12AK33A. The authors acknowledge Ami Hannon for help with the gas
sensing measurements.
NR 27
TC 1
Z9 1
U1 15
U2 29
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD MAR 21
PY 2016
VL 108
IS 12
AR 123103
DI 10.1063/1.4943792
PG 4
WC Physics, Applied
SC Physics
GA DI2SD
UT WOS:000373348000036
ER
PT J
AU Farnhill, HJ
Drew, JE
Barentsen, G
Gonzalez-Solares, EA
AF Farnhill, H. J.
Drew, J. E.
Barentsen, G.
Gonzalez-Solares, E. A.
TI Calibrated and completeness-corrected optical stellar density maps of
the northern Galactic plane
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE atlases; dust, extinction; Galaxy: disc; Galaxy: stellar content;
Galaxy: structure
ID DIGITAL SKY SURVEY; H-ALPHA SURVEY; MILKY-WAY; DATA RELEASE; STAR
COUNTS; EXTINCTION; IPHAS; PHOTOMETRY; CONFUSION; CLUSTERS
AB Following on from the second release of calibrated photometry from IPHAS, the INT/WFC Photometric H alpha Survey of the Northern Galactic Plane, we present incompleteness-corrected stellar density maps in the r and i photometric bands. These have been computed to a range of limiting magnitudes reaching to 20th magnitude in r and 19th in i (Vega system), and with different angular resolutions - the highest resolution available being 1 arcmin(2). The maps obtained cover 94 per cent of the 1800 square degree IPHAS footprint, spanning the Galactic latitude range, -5 degrees < b < +5 degrees, north of the celestial equator. The corrections for incompleteness, due to confusion and sensitivity loss at the faint limit, have been deduced by the method of artificial source injection. The presentation of this method is preceded by a discussion of other more approximate methods of determining completeness. Our method takes full account of position-dependent seeing and source ellipticity in the survey data base. The application of the star counts to testing reddened Galactic disc models is previewed by a comparison with predicted counts along three constant-longitude cuts at l similar or equal to 30 degrees, 90 degrees and 175 degrees : some overprediction of the most heavily reddened l similar or equal to 30 degrees counts is found, alongside good agreement at l similar or equal to 90 degrees and 175 degrees.
C1 [Farnhill, H. J.; Drew, J. E.; Barentsen, G.] Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England.
[Barentsen, G.] NASA, Ames Res Ctr, Mail Stop 245-30, Moffett Field, CA 94035 USA.
[Gonzalez-Solares, E. A.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 OHA, England.
RP Farnhill, HJ; Drew, JE (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England.
EM hywel@farnhill.io; j.drew@herts.ac.uk
OI Drew, Janet/0000-0003-1192-7082
FU Science & Technology Facilities Council (STFC) of the United Kingdom
[ST/J001333/1]; STFC
FX The bandmerged DR2 catalogue underpinning this work was assembled at the
Centre for Astrophysics Research, University of Hertfordshire, supported
by a grant awarded by the Science & Technology Facilities Council (STFC)
of the United Kingdom [ST/J001333/1]. HJF also acknowledges the receipt
of a PhD studentship funded by the STFC.
NR 38
TC 0
Z9 0
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 21
PY 2016
VL 457
IS 1
BP 642
EP 665
DI 10.1093/mnras/stv2994
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH2FM
UT WOS:000372599600045
ER
PT J
AU Suchyta, E
Huff, EM
Aleksic, J
Melchior, P
Jouvel, S
MacCrann, N
Ross, AJ
Crocce, M
Gaztanaga, E
Honscheid, K
Leistedt, B
Peiris, HV
Rykoff, ES
Sheldon, E
Abbott, T
Abdalla, FB
Allam, S
Banerji, M
Benoit-Levy, A
Bertin, E
Burke, DL
Burke, DL
Rosell, AC
Kind, MC
Carretero, J
Cunha, CE
D'Andrea, CB
da Costa, LN
Depoy, DL
Desai, S
Diehl, HT
Dietrich, JP
Doel, P
Eifler, TF
Estrada, J
Evrard, AE
Flaugher, B
Fosalba, P
Frieman, J
Gerdes, DW
Gruen, D
Gruendl, RA
James, DJ
Jarvis, M
Kuehn, K
Kuropatkin, N
Lahav, O
Lima, M
Maia, MAG
March, M
Marshall, JL
Miller, CJ
Miquel, R
Neilsen, E
Nichol, RC
Nord, B
Ogando, R
Percival, WJ
Reil, K
Roodman, A
Sako, M
Sanchez, E
Scarpine, V
Sevilla-Noarbe, I
Smith, RC
Soares-Santos, M
Sobreira, F
Swanson, MEC
Tarle, G
Thaler, J
Thomas, D
Vikram, V
Walker, AR
Wechsler, RH
Zhang, Y
AF Suchyta, E.
Huff, E. M.
Aleksic, J.
Melchior, P.
Jouvel, S.
MacCrann, N.
Ross, A. J.
Crocce, M.
Gaztanaga, E.
Honscheid, K.
Leistedt, B.
Peiris, H. V.
Rykoff, E. S.
Sheldon, E.
Abbott, T.
Abdalla, F. B.
Allam, S.
Banerji, M.
Benoit-Levy, A.
Bertin, E.
Brooks, D.
Burke, D. L.
Carnero Rosell, A.
Carrasco Kind, M.
Carretero, J.
Cunha, C. E.
D'Andrea, C. B.
da Costa, L. N.
DePoy, D. L.
Desai, S.
Diehl, H. T.
Dietrich, J. P.
Doel, P.
Eifler, T. F.
Estrada, J.
Evrard, A. E.
Flaugher, B.
Fosalba, P.
Frieman, J.
Gerdes, D. W.
Gruen, D.
Gruendl, R. A.
James, D. J.
Jarvis, M.
Kuehn, K.
Kuropatkin, N.
Lahav, O.
Lima, M.
Maia, M. A. G.
March, M.
Marshall, J. L.
Miller, C. J.
Miquel, R.
Neilsen, E.
Nichol, R. C.
Nord, B.
Ogando, R.
Percival, W. J.
Reil, K.
Roodman, A.
Sako, M.
Sanchez, E.
Scarpine, V.
Sevilla-Noarbe, I.
Smith, R. C.
Soares-Santos, M.
Sobreira, F.
Swanson, M. E. C.
Tarle, G.
Thaler, J.
Thomas, D.
Vikram, V.
Walker, A. R.
Wechsler, R. H.
Zhang, Y.
CA DES Collaboration
TI No galaxy left behind: accurate measurements with the faintest objects
in the Dark Energy Survey
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; methods: miscellaneous; techniques: image
processing; galaxies: statistics
ID DIGITAL SKY SURVEY; REDSHIFT-SPACE DISTORTIONS; SCIENCE VERIFICATION
DATA; PHOTOMETRIC REDSHIFTS; WIDE-FIELD; SDSS-III; CALIBRATION; COSMOS;
SELECTION; UNCERTAINTIES
AB Accurate statistical measurement with large imaging surveys has traditionally required throwing away a sizable fraction of the data. This is because most measurements have relied on selecting nearly complete samples, where variations in the composition of the galaxy population with seeing, depth, or other survey characteristics are small. We introduce a new measurement method that aims to minimize this wastage, allowing precision measurement for any class of detectable stars or galaxies. We have implemented our proposal in BALROG, software which embeds fake objects in real imaging to accurately characterize measurement biases. We demonstrate this technique with an angular clustering measurement using Dark Energy Survey (DES) data. We first show that recovery of our injected galaxies depends on a variety of survey characteristics in the same way as the real data. We then construct a flux-limited sample of the faintest galaxies in DES, chosen specifically for their sensitivity to depth and seeing variations. Using the synthetic galaxies as randoms in the Landy-Szalay estimator suppresses the effects of variable survey selection by at least two orders of magnitude. With this correction, our measured angular clustering is found to be in excellent agreement with that of a matched sample from much deeper, higher resolution space-based Cosmological Evolution Survey (COSMOS) imaging; over angular scales of 0 degrees.004 < theta < 0 degrees.2, we find a best-fitting scaling amplitude between the DES and COSMOS measurements of 1.00 +/- 0.09. We expect this methodology to be broadly useful for extending measurements' statistical reach in a variety of upcoming imaging surveys.
C1 [Suchyta, E.; Huff, E. M.; Melchior, P.; Honscheid, K.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Suchyta, E.; Huff, E. M.; Melchior, P.; Ross, A. J.; Honscheid, K.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Aleksic, J.; Carretero, J.; Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[Jouvel, S.; Leistedt, B.; Peiris, H. V.; Abdalla, F. B.; Brooks, D.; Doel, P.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
[MacCrann, N.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England.
[Crocce, M.; Gaztanaga, E.; Carretero, J.; Fosalba, P.] CSIC, IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain.
[Rykoff, E. S.; Burke, D. L.; Cunha, C. E.; Roodman, A.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA.
[Rykoff, E. S.; Burke, D. L.; Reil, K.; Roodman, A.; Wechsler, R. H.] Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA.
[Abbott, T.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile.
[Abdalla, F. B.; Estrada, J.] Rhodes Univ, Dept Phys Elect, POB 94, ZA-6140 Grahamstown, South Africa.
[Allam, S.; Diehl, H. T.; Flaugher, B.; Frieman, J.; Kuropatkin, N.; Neilsen, E.; Nord, B.; Scarpine, V.; Soares-Santos, M.; Sobreira, F.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA.
[Banerji, M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Banerji, M.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England.
[Bertin, E.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Bertin, E.] Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Carnero Rosell, A.; da Costa, L. N.; Lima, M.; Maia, M. A. G.; Ogando, R.; Sobreira, F.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921 Rio De Janeiro, RJ, Brazil.
[Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921 Rio De Janeiro, RJ, Brazil.
[Carrasco Kind, M.; Gruendl, R. A.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Carrasco Kind, M.; Gruendl, R. A.; Swanson, M. E. C.] Univ Illinois, Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA.
[D'Andrea, C. B.; Nichol, R. C.; Percival, W. J.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[DePoy, D. L.; Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[DePoy, D. L.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Desai, S.; Dietrich, J. P.] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany.
[Desai, S.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Dietrich, J. P.; Gruen, D.] Univ Munich, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Eifler, T. F.; Jarvis, M.; March, M.; Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Eifler, T. F.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Evrard, A. E.; Gerdes, D. W.; Miller, C. J.; Tarle, G.; Zhang, Y.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Gruen, D.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, Brazil.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
[Sanchez, E.; Sevilla-Noarbe, I.] CIEMAT, E-28040 Madrid, Spain.
[Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA.
[Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA.
[Wechsler, R. H.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA.
RP Suchyta, E; Huff, EM (reprint author), Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA.; Suchyta, E; Huff, EM (reprint author), Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
EM eric.d.suchyta@gmail.com; emhuff@gmail.com
RI Lima, Marcos/E-8378-2010; Fosalba Vela, Pablo/I-5515-2016; Ogando,
Ricardo/A-1747-2010; Sobreira, Flavia/F-4168-2015; Gaztanaga,
Enrique/L-4894-2014;
OI Ogando, Ricardo/0000-0003-2120-1154; Sobreira,
Flavia/0000-0002-7822-0658; Gaztanaga, Enrique/0000-0001-9632-0815;
Suchyta, Eric/0000-0002-7047-9358; Carrasco Kind,
Matias/0000-0002-4802-3194; Abdalla, Filipe/0000-0003-2063-4345
FU Ohio State University Graduate Presidential Fellowship; CCAPP
postdoctoral fellowship; MINECO [FPA2012-39684, AYA2012-39559,
ESP2013-48274, FPA2013-47986]; US Department of Energy
[DE-FG02-91ER40690]; US National Science Foundation; Ministry of Science
and Education of Spain; Science and Technology Facilities Council of the
United Kingdom; Higher Education Funding Council for England; National
Center for Supercomputing Applications at the University of Illinois at
Urbana-Champaign; Kavli Institute of Cosmological Physics at the
University of Chicago; Center for Cosmology and Astro-Particle Physics
at The Ohio State University; Mitchell Institute for Fundamental Physics
and Astronomy at Texas AM University; Financiadora de Estudos e
Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do
Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e
Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche
Forschungsgemeinschaft; DES; National Science Foundation [AST-1138766];
Argonne National Laboratory; University of California at Santa Cruz;
University of Cambridge; Centro de Investigaciones Energeticas;
Medioambientales y Tecnologicas-Madrid; University of Chicago;
University College London; DES-Brazil Consortium; University of
Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi
National Accelerator Laboratory; University of Illinois at
Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut
de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory;
Ludwig-Maximilians Universitat Munchen; associated Excellence Cluster
Universe; University of Michigan; National Optical Astronomy
Observatory; University of Nottingham; Ohio State University; University
of Pennsylvania; University of Portsmouth; SLAC National Accelerator
Laboratory; Stanford University; University of Sussex; Texas AM
University; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European
Research Council under the European Union [240672, 291329, 306478]
FX ES is supported by an Ohio State University Graduate Presidential
Fellowship. EMH is funded by a CCAPP postdoctoral fellowship. JA is
partially supported by MINECO under grant FPA2012-39684. PM is supported
by the US Department of Energy under Contract No. DE-FG02-91ER40690.r
Funding for the DES Projects has been provided by the US Department of
Energy, the US National Science Foundation, the Ministry of Science and
Education of Spain, the Science and Technology Facilities Council of the
United Kingdom, the Higher Education Funding Council for England, the
National Center for Supercomputing Applications at the University of
Illinois at Urbana-Champaign, the Kavli Institute of Cosmological
Physics at the University of Chicago, the Center for Cosmology and
Astro-Particle Physics at The Ohio State University, the Mitchell
Institute for Fundamental Physics and Astronomy at Texas A&M University,
Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de
Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia,
Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the
Collaborating Institutions in the DES. The DESDM system is supported by
the National Science Foundation under Grant Number AST-1138766.r The
Collaborating Institutions are Argonne National Laboratory, the
University of California at Santa Cruz, the University of Cambridge,
Centro de Investigaciones Energeticas, Medioambientales y
Tecnologicas-Madrid, the University of Chicago, University College
London, the DES-Brazil Consortium, the University of Edinburgh, the
Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National
Accelerator Laboratory, the University of Illinois at Urbana-Champaign,
the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica
d'Altes Energies, Lawrence Berkeley National Laboratory, the
Ludwig-Maximilians Universitat Munchen and the associated Excellence
Cluster Universe, the University of Michigan, the National Optical
Astronomy Observatory, the University of Nottingham, The Ohio State
University, the University of Pennsylvania, the University of
Portsmouth, SLAC National Accelerator Laboratory, Stanford University,
the University of Sussex, and Texas A&M University.r The DES
participants from Spanish institutions are partially supported by MINECO
under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de
Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results
has received funding from the European Research Council under the
European Unions Seventh Framework Programme (FP7/2007-2013) including
ERC grant agreements 240672, 291329, and 306478.
NR 66
TC 7
Z9 7
U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 21
PY 2016
VL 457
IS 1
BP 786
EP 808
DI 10.1093/mnras/stv2953
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH2FM
UT WOS:000372599600054
ER
PT J
AU Weston, JHS
Sokoloski, JL
Metzger, BD
Zheng, Y
Chomiuk, L
Krauss, MI
Linford, JD
Nelson, T
Mioduszewski, AJ
Rupen, MP
Finzell, T
Mukai, K
AF Weston, Jennifer H. S.
Sokoloski, J. L.
Metzger, Brian D.
Zheng, Yong
Chomiuk, Laura
Krauss, Miriam I.
Linford, Justin D.
Nelson, Thomas
Mioduszewski, Amy J.
Rupen, Michael P.
Finzell, Tom
Mukai, Koji
TI Non-thermal radio emission from colliding flows in classical nova V1723
Aql
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: general; novae, cataclysmic variables; stars: variables:
general; white dwarfs; stars: winds, outflows; radio continuum: stars
ID RECURRENT NOVA; MASS-LOSS; PARTICLE-ACCELERATION; THERMAL EMISSION;
VULPECULAE 1984; RAY SOURCES; HOT STARS; OUTBURST; REMNANT; EJECTA
AB The importance of shocks in nova explosions has been highlighted by Fermi's discovery of gamma-ray-producing novae. Over three years of multiband Very Large Array radio observations of the 2010 nova V1723 Aql show that shocks between fast and slow flows within the ejecta led to the acceleration of particles and the production of synchrotron radiation. Soon after the start of the eruption, shocks in the ejecta produced an unexpected radio flare, resulting in a multipeaked radio light curve. The emission eventually became consistent with an expanding thermal remnant with mass 2 x 10(-4) M-circle dot and temperature 10(4) K. However, during the first two months, the greater than or similar to 10(6) K brightness temperature at low frequencies was too high to be due to thermal emission from the small amount of X-ray-producing shock-heated gas. Radio imaging showed structures with velocities of 400 km s(-1) (d/6 kpc) in the plane of the sky, perpendicular to a more elongated 1500 km s(-1) (d/6 kpc) flow. The morpho-kinematic structure of the ejecta from V1723 Aql appears similar to nova V959 Mon, where collisions between a slow torus and a faster flow collimated the fast flow and gave rise to gamma-ray-producing shocks. Optical spectroscopy and X-ray observations of V1723 Aql during the radio flare are consistent with this picture. Our observations support the idea that shocks in novae occur when a fast flow collides with a slow collimating torus. Such shocks could be responsible for hard X-ray emission, gamma-ray production, and double-peaked radio light curves from some classical novae.
C1 [Weston, Jennifer H. S.; Sokoloski, J. L.; Metzger, Brian D.; Zheng, Yong] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Chomiuk, Laura; Linford, Justin D.; Finzell, Tom] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Krauss, Miriam I.; Mioduszewski, Amy J.] Natl Radio Astron Observ, POB O,1003 Lopezville Rd, Socorro, NM 87801 USA.
[Nelson, Thomas] Univ Minnesota, Sch Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA.
[Rupen, Michael P.] Natl Res Council Canada, Domin Radio Astrophys Observ, Herzberg Astron & Astrophys Programs, POB 248, Penticton, BC V2A 6J9, Canada.
[Mukai, Koji] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Mukai, Koji] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Mukai, Koji] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
RP Weston, JHS; Sokoloski, JL (reprint author), Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
EM jennifer@astro.columbia.edu; jeno@astro.columbia.edu
OI Zheng, Yong/0000-0003-4158-5116
FU NSF [AST-1211778, AST-1410950]; NRAO [NRAO 343777]; NASA Fermi grant
[NNX14AQ68G]; Alfred P. Sloan Foundation; NASA Fermi Guest Investigator
grant [NNH13ZDA001N-FERMI]; NASA award [NNX13A091G]
FX We thank NRAO for its generous allocation of time which made this work
possible. The NRAO is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc. JW
and JLS acknowledge support from NSF award AST-1211778. JW was supported
in part by a Student Observing Support award from NRAO (NRAO 343777).
BDM gratefully acknowledges support from NASA Fermi grant NNX14AQ68G,
NSF grant AST-1410950, and the Alfred P. Sloan Foundation. LC, JL, and
TF are supported by NASA Fermi Guest Investigator grant
NNH13ZDA001N-FERMI. TN was supported in part by NASA award NNX13A091G.
We thank Benson Way for assistance with Fig. 4.
NR 48
TC 3
Z9 3
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 21
PY 2016
VL 457
IS 1
BP 887
EP 901
DI 10.1093/mnras/stv3019
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH2FM
UT WOS:000372599600061
ER
PT J
AU Shu, YP
Bolton, AS
Moustakas, LA
Stern, D
Dey, A
Brownstein, JR
Burles, S
Spinrad, H
AF Shu, Yiping
Bolton, Adam S.
Moustakas, Leonidas A.
Stern, Daniel
Dey, Arjun
Brownstein, Joel R.
Burles, Scott
Spinrad, Hyron
TI KILOPARSEC MASS/LIGHT OFFSETS IN THE GALAXY PAIR-Ly alpha EMITTER LENS
SYSTEM SDSS J1011+0143
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; galaxies: individual (SDSS J1011+0143); galaxies:
interactions; gravitational lensing: strong; techniques: image
processing
ID SPECTROSCOPICALLY SELECTED SAMPLE; INTERACTION CROSS-SECTION; MATTER
SELF-INTERACTIONS; MASS-DENSITY PROFILE; COLD DARK-MATTER; ACS SURVEY;
ABELL 3827; CLUSTER 1E-0657-56; ADAPTIVE OPTICS; RX J1347.5-1145
AB We report the discovery of significant mass/light offsets in the strong gravitational lensing system SDSS J1011 + 0143. We use the high-resolution Hubble Space Telescope (HST) F555W- and F814W-band imaging and Sloan Digital Sky Survey (SDSS) spectroscopy of this system, which consists of a close galaxy pair with a projected separation of approximate to 4.2 kpc at z(lens) similar to 0.331 lensing an Ly alpha emitter (LAE) at z(source) = 2.701. Comparisons between the mass peaks inferred from lens models and light peaks from HST imaging data reveal significant spatial mass/light offsets as large as 1.72 +/- 0.24 +/- 0.34. kpc in both filter bands. Such large mass/light offsets, not seen in isolated field lens galaxies and relaxed galaxy groups, may be related to the interactions between the two lens galaxies. The detected mass/light offsets can potentially serve as an important test for the self-interacting dark matter model. However, other mechanisms such as dynamical friction on spatially differently distributed dark matter and stars could produce similar offsets. Detailed hydrodynamical simulations of galaxy-galaxy interactions with self-interacting dark matter could accurately quantify the effects of different mechanisms. The background LAE is found to contain three distinct star-forming knots with characteristic sizes from 116 to 438 pc. It highlights the power of strong gravitational lensing in probing the otherwise too faint and unresolved structures of distance objects below subkiloparsec or even 100 pc scales through its magnification effect.
C1 [Shu, Yiping] Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100012, Peoples R China.
[Shu, Yiping; Bolton, Adam S.; Brownstein, Joel R.] Univ Utah, Dept Phys & Astron, 115 South 1400 East, Salt Lake City, UT 84112 USA.
[Moustakas, Leonidas A.; Stern, Daniel] CALTECH, Jet Prop Lab, MS 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Burles, Scott] Cutler Grp LP, 101 Montgomery St,Suite 700, San Francisco, CA 94104 USA.
[Spinrad, Hyron] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Shu, YP (reprint author), Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100012, Peoples R China.; Shu, YP (reprint author), Univ Utah, Dept Phys & Astron, 115 South 1400 East, Salt Lake City, UT 84112 USA.
EM yiping.shu@nao.cas.cn
FU Center for High Performance Computing at the University of Utah;
National Optical Astronomy Observatory (NOAO); NASA [10831]; Alfred P.
Sloan Foundation; National Science Foundation; U.S. Department of
Energy; National Aeronautics and Space Administration; Japanese
Monbukagakusho; Max Planck Society; Higher Education Funding Council for
England
FX We thank the anonymous referee for helpful comments. The support and
resources from the Center for High Performance Computing at the
University of Utah are gratefully acknowledged. The work of L.A.M. and
D.S. was carried out at Jet Propulsion Laboratory, California Institute
of Technology, under a contract with NASA. A.D.'s research was supported
by the National Optical Astronomy Observatory (NOAO). NOAO is operated
by the Association of Universities for Research in Astronomy (AURA),
Inc., under a cooperative agreement with the National Science
Foundation. Support for program #10831 was provided by NASA through a
grant from the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS 5-26555.; Funding for the SDSS and SDSS-II has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Science Foundation, the U.S. Department of
Energy, the National Aeronautics and Space Administration, the Japanese
Monbukagakusho, the Max Planck Society, and the Higher Education Funding
Council for England. The SDSS Web site is http://www.sdss.org/.
NR 70
TC 4
Z9 4
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 43
DI 10.3847/0004-637X/820/1/43
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DU4IC
UT WOS:000382175300001
ER
PT J
AU Chemyakin, E
Burton, S
Kolgotin, A
Muller, D
Hostetler, C
Ferrare, R
AF Chemyakin, Eduard
Burton, Sharon
Kolgotin, Alexei
Muller, Detlef
Hostetler, Chris
Ferrare, Richard
TI Retrieval of aerosol parameters from multiwavelength lidar:
investigation of the underlying inverse mathematical problem
SO APPLIED OPTICS
LA English
DT Article
ID MICROPHYSICAL PARTICLE PARAMETERS; PRINCIPAL COMPONENT ANALYSIS; RAMAN
LIDAR; TROPOSPHERIC AEROSOL; OPTICAL-PROPERTIES; REGULARIZATION;
EXTINCTION; BACKSCATTER
AB We present an investigation of some important mathematical and numerical features related to the retrieval of microphysical parameters [complex refractive index, single-scattering albedo, effective radius, total number, surface area, and volume concentrations] of ambient aerosol particles using multiwavelength Raman or high-spectral-resolution lidar. Using simple examples, we prove the non-uniqueness of an inverse solution to be the major source of the retrieval difficulties. Some theoretically possible ways of partially compensating for these difficulties are offered. For instance, an increase in the variety of input data via combination of lidar and certain passive remote sensing instruments will be helpful to reduce the error of estimation of the complex refractive index. We also demonstrate a significant interference between Aitken and accumulation aerosol modes in our inversion algorithm, and confirm that the solutions can be better constrained by limiting the particle radii. Applying a combination of an analytical approach and numerical simulations, we explain the statistical behavior of the microphysical size parameters. We reveal and clarify why the total surface area concentration is consistent even in the presence of non-unique solution sets and is on average the most stable parameter to be estimated, as long as at least one extinction optical coefficient is employed. We find that for selected particle size distributions, the total surface area and volume concentrations can be quickly retrieved with fair precision using only single extinction coefficients in a simple arithmetical relationship. (C) 2016 Optical Society of America
C1 [Chemyakin, Eduard; Muller, Detlef] NASA, Sci Syst & Applicat Inc, Langley Res Ctr, Mail Stop 475, Hampton, VA 23681 USA.
[Burton, Sharon; Hostetler, Chris; Ferrare, Richard] NASA, Langley Res Ctr, Mail Stop 401A, Hampton, VA 23681 USA.
[Kolgotin, Alexei] AM Prokhorov Gen Phys Inst, Phys Instrumentat Ctr, Moscow 142190, Russia.
[Muller, Detlef] Univ Hertfordshire, Coll Lane, Hatfield AL10 9AB, Herts, England.
RP Chemyakin, E (reprint author), NASA, Sci Syst & Applicat Inc, Langley Res Ctr, Mail Stop 475, Hampton, VA 23681 USA.
EM eduard.chemyakin@ssaihq.com
NR 26
TC 3
Z9 3
U1 0
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD MAR 20
PY 2016
VL 55
IS 9
BP 2188
EP 2202
DI 10.1364/AO.55.002188
PG 15
WC Optics
SC Optics
GA DI3LO
UT WOS:000373400400011
PM 27140552
ER
PT J
AU Ackermann, M
Ajello, M
An, H
Baldini, L
Barbiellini, G
Bastieri, D
Bellazzini, R
Bissaldi, E
Blandford, RD
Bonino, R
Bregeon, J
Britto, RJ
Bruel, P
Buehler, R
Caliandro, GA
Cameron, RA
Caragiulo, M
Caraveo, PA
Cavazzuti, E
Cecchi, C
Charles, E
Chekhtman, A
Chiaro, G
Ciprini, S
Cohen-Tanugi, J
Costanza, F
Cutini, S
D'Ammando, F
de Angelis, A
de Palma, F
Desiante, R
Di Mauro, M
Di Venere, L
Dominiguez, A
Drell, PS
Favuzzi, C
Fegan, SJ
Ferrara, EC
Finke, J
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Giordano, F
Giroletti, M
Green, D
Grenier, IA
Guiriec, S
Horan, D
Johannesson, G
Katsuragawa, M
Kuss, M
Larsson, S
Latronico, L
Li, J
Li, L
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Magill, J
Maldera, S
Manfreda, A
Mayer, M
Mazziotta, MN
Michelson, PF
Mirabal, N
Mitthumsiri, W
Mizuno, T
Monzani, ME
Morselli, A
Moskalenko, IV
Negro, M
Nuss, E
Ohsugi, T
Okada, C
Orlando, E
Paneque, D
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, O
Rau, A
Romani, RW
Schady, P
Sgro, C
Simone, D
Siskind, EJ
Spada, F
Spandre, G
Spinelli, P
Stern, D
Takahashi, H
Thayer, JB
Torres, DF
Tosti, G
Troja, E
Vianello, G
Wood, KS
Wood, M
AF Ackermann, M.
Ajello, M.
An, H.
Baldini, L.
Barbiellini, G.
Bastieri, D.
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bonino, R.
Bregeon, J.
Britto, R. J.
Bruel, P.
Buehler, R.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Caraveo, P. A.
Cavazzuti, E.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiaro, G.
Ciprini, S.
Cohen-Tanugi, J.
Costanza, F.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Desiante, R.
Di Mauro, M.
Di Venere, L.
Dominiguez, A.
Drell, P. S.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Finke, J.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Giordano, F.
Giroletti, M.
Green, D.
Grenier, I. A.
Guiriec, S.
Horan, D.
Johannesson, G.
Katsuragawa, M.
Kuss, M.
Larsson, S.
Latronico, L.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Magill, J.
Maldera, S.
Manfreda, A.
Mayer, M.
Mazziotta, M. N.
Michelson, P. F.
Mirabal, N.
Mitthumsiri, W.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Negro, M.
Nuss, E.
Ohsugi, T.
Okada, C.
Orlando, E.
Paneque, D.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, O.
Rau, A.
Romani, R. W.
Schady, P.
Sgro, C.
Simone, D.
Siskind, E. J.
Spada, F.
Spandre, G.
Spinelli, P.
Stern, D.
Takahashi, H.
Thayer, J. B.
Torres, D. F.
Tosti, G.
Troja, E.
Vianello, G.
Wood, K. S.
Wood, M.
TI CONTEMPORANEOUS BROADBAND OBSERVATIONS OF THREE HIGH-REDSHIFT BL LAC
OBJECTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: general; BL Lacertae objects: individual (3FGL
J0022.1-1855, 3FGL J0630.9-2406; 3FGL J0811.2-7529); galaxies: active;
radiation mechanisms: non-thermal
ID EXTRAGALACTIC BACKGROUND LIGHT; LARGE-AREA TELESCOPE; GAMMA-RAY SPECTRA;
ACTIVE GALACTIC NUCLEI; GALAXY SURVEY DATA; LACERTAE OBJECTS;
MULTIWAVELENGTH OBSERVATIONS; PHYSICAL-PROPERTIES; ENERGY-DISTRIBUTION;
BRIGHT BLAZARS
AB We have collected broadband spectral energy distributions (SEDs) of three BL Lac objects 3FGL J0022.1-1855 (z = 0.689), 3FGL J0630.9-2406 (z greater than or similar to 1.239), and 3FGL J0811.2-7529 (z = 0.774), detected by Fermi with relatively flat gigaelectronvolt spectra. By observing simultaneously in the near-infrared to hard X-ray band, we can well characterize the high end of the synchrotron component of the SED. Thus, fitting the SEDs to synchro-Compton models of the dominant emission from the relativistic jet, we can constrain the underlying particle properties and predict the shape of the gigaelectronvolt Compton component. Standard extragalactic background light (EBL) models explain the high-energy absorption well, with poorer fits for high-ultraviolet models. The fits show clear evidence for EBL absorption in the Fermi spectrum of our highest-redshift source 3FGL J0630.9-2406. While synchrotron self-Compton models adequately describe the SEDs, the situation may be complicated by possible external Compton components. For 3FGL J0811.2-7529, we also discover a nearby serendipitous source in the X-ray data, which is almost certainly another lower synchrotron peak frequency (nu(sy)(pk)) BL Lac, that may contribute flux in the Fermi band. Since our sources are unusual high-luminosity, moderate nu(sy)(pk) BL Lacs, we compare these quantities and the Compton dominance, the ratio of peak inverse Compton to peak synchrotron luminosities (L-pk(IC)/L-pk(sy)), with those of the full Fermi BL Lac population.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.] DESY, Deutsch Elekt Synchrotron, D-12738 Zeuthen, Germany.
[Ajello, M.; Dominiguez, A.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[An, H.; Baldini, L.; Blandford, R. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Di Mauro, M.; Drell, P. S.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Porter, T. A.; Reimer, O.; Romani, R. W.; Thayer, J. B.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[An, H.; Baldini, L.; Blandford, R. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Di Mauro, M.; Drell, P. S.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Porter, T. A.; Reimer, O.; Romani, R. W.; Thayer, J. B.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.; Bellazzini, R.; Chekhtman, A.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Chiaro, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bissaldi, E.; Caragiulo, M.; Costanza, F.; de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Simone, D.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bonino, R.; Desiante, R.; Latronico, L.; Maldera, S.; Negro, M.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bonino, R.; Negro, M.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier, Lab Univ & Particules Montpellier, CNRS, IN2P3, F-34059 Montpellier, France.
[Britto, R. J.] Univ Johannesburg, Dept Phys, POB 524,Auckland Pk, ZA-2006 Johannesburg, South Africa.
[Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Caraveo, P. A.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] ASI Sci Data Ctr, I-00133 Rome, Italy.
[Cecchi, C.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA.
[Cutini, S.] Osserv Astron Roma, INAF, I-00040 Rome, Italy.
[D'Ammando, F.; Giroletti, M.] Inst Radioastron, INAF, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy.
[de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Ferrara, E. C.; Green, D.; Guiriec, S.; Mirabal, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Finke, J.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Green, D.; Magill, J.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Green, D.; Magill, J.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Grenier, I. A.; Troja, E.] Univ Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU CNRS, F-91191 Gif Sur Yvette, France.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Katsuragawa, M.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
[Larsson, S.; Li, L.] KTH Royal Inst Technol, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
[Larsson, S.; Li, L.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Li, J.; Torres, D. F.] Inst Space Sci IEEC CSIC, Campus UAB, E-08193 Barcelona, Spain.
[Mitthumsiri, W.] Mahidol Univ, Fac Sci, Dept Phys, Bangkok 10400, Thailand.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Okada, C.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Rau, A.; Schady, P.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Stern, D.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
RP An, H (reprint author), Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.; An, H (reprint author), Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
EM hjans@stanford.edu
RI Moskalenko, Igor/A-1301-2007; Bissaldi, Elisabetta/K-7911-2016; Reimer,
Olaf/A-3117-2013; Orlando, E/R-5594-2016; Bonino, Raffaella/S-2367-2016;
Torres, Diego/O-9422-2016; Di Venere, Leonardo/C-7619-2017;
OI Ajello, Marco/0000-0002-6584-1703; Sgro', Carmelo/0000-0001-5676-6214;
Moskalenko, Igor/0000-0001-6141-458X; Bissaldi,
Elisabetta/0000-0001-9935-8106; Gargano, Fabio/0000-0002-5055-6395;
Pesce-Rollins, Melissa/0000-0003-1790-8018; An,
Hongjun/0000-0002-6389-9012; DI MAURO, MATTIA/0000-0003-2759-5625;
Reimer, Olaf/0000-0001-6953-1385; Torres, Diego/0000-0002-1522-9065; Di
Venere, Leonardo/0000-0003-0703-824X; Mazziotta, Mario
Nicola/0000-0001-9325-4672
FU NASA [NNG08FD60C, NAS5-00147]; National Aeronautics and Space
Administration; Kavli Institute for Particle Astrophysics and Cosmology
(KIPAC); DFG [HA 1850/28-1]
FX This work was supported under NASA Contract No. NNG08FD60C and made use
of data from the NuSTAR mission, a project led by the California
Institute of Technology, managed by the Jet Propulsion Laboratory, and
funded by the National Aeronautics and Space Administration. We thank
the NuSTAR Operations, Software, and Calibration teams for support with
the execution and analysis of these observations. This research has made
use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed
by the ASI Science Data Center (ASDC, Italy) and the California
Institute of Technology (USA).r H.A. acknowledges support provided by
the NASA-sponsored Fermi Contract NAS5-00147 and by the Kavli Institute
for Particle Astrophysics and Cosmology (KIPAC). Part of the funding for
GROND (both hardware and personnel) was generously granted from the
Leibniz Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1).
NR 61
TC 1
Z9 1
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 72
DI 10.3847/0004-637X/820/1/72
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000071
ER
PT J
AU Apai, D
Kasper, M
Skemer, A
Hanson, JR
Lagrange, AM
Biller, BA
Bonnefoy, M
Buenzli, E
Vigan, A
AF Apai, Daniel
Kasper, Markus
Skemer, Andrew
Hanson, Jake R.
Lagrange, Anne-Marie
Biller, Beth A.
Bonnefoy, Mickael
Buenzli, Esther
Vigan, Arthur
TI HIGH-CADENCE, HIGH-CONTRAST IMAGING FOR EXOPLANET MAPPING: OBSERVATIONS
OF THE HR 8799 PLANETS WITH VLT/SPHERE SATELLITE-SPOT-CORRECTED RELATIVE
PHOTOMETRY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: observational; planetary systems; planets and satellites:
atmospheres; planets and satellites: gaseous planets; planets and
satellites: individual (HR 8799); techniques: photometric
ID HUBBLE-SPACE-TELESCOPE; BROWN DWARFS; BETA-PICTORIS; SPECTROSCOPIC
VARIABILITY; EVOLVING WEATHER; LIGHT CURVES; T DWARFS; MU-M; YOUNG;
ASTROMETRY
AB Time-resolved photometry is an important new probe of the physics of condensate clouds in extrasolar planets and brown dwarfs. Extreme adaptive optics systems can directly image planets, but precise brightness measurements are challenging. We present VLT/SPHERE high-contrast, time-resolved broad H-band near-infrared photometry for four exoplanets in the HR 8799 system, sampling changes from night to night over five nights with relatively short integrations. The photospheres of these four planets are often modeled by patchy clouds and may show large-amplitude rotational brightness modulations. Our observations provide high-quality images of the system. We present a detailed performance analysis of different data analysis approaches to accurately measure the relative brightnesses of the four exoplanets. We explore the information in satellite spots and demonstrate their use as a proxy for image quality. While the brightness variations of the satellite spots are strongly correlated, we also identify a second-order anti-correlation pattern between the different spots. Our study finds that KLIP reduction based. on principal components analysis with satellite-spot-modulated artificial-planet-injection-based photometry leads to a significant (similar to 3x) gain in photometric accuracy over standard aperture-based photometry and reaches 0.1 mag per point accuracy for our data set, the signal-to-noise ratio of which is limited by small field rotation. Relative planet-to-planet photometry can be compared between nights, enabling observations spanning multiple nights to probe variability. Recent high-quality relative H-band photometry of the b-c planet pair agrees to about 1%.
C1 [Apai, Daniel; Skemer, Andrew; Hanson, Jake R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Kasper, Markus] European So Observ, Karl Schwarzschild Str 2, Garching, Germany.
[Lagrange, Anne-Marie; Bonnefoy, Mickael] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Biller, Beth A.] Univ Edinburgh, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Buenzli, Esther] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Vigan, Arthur] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France.
[Apai, Daniel] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Apai, Daniel; Skemer, Andrew] NASA, Earths Other Solar Syst Team, Nexus Exoplanet Syst Sci, Washington, DC USA.
[Bonnefoy, Mickael] CNRS, IPAG, F-38000 Grenoble, France.
RP Apai, D (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
EM apai@arizona.edu
OI Vigan, Arthur/0000-0002-5902-7828
FU Swiss National Science Foundation (SNSF); ESO Telescopes at the La Silla
Paranal Observatory [60.A-9352(A)]; NASA's Science Mission Directorate
FX We thank the anonymous referee for the detailed, constructive, and
prompt reviews that helped to improve the clarity of the manuscript. We
are grateful to the SPHERE consortium for their hard work in building
such a capable instrument, the ESO astronomers for carrying out the
observations, and the ESO User Support group for their assistance with
the planning of the observations. E.B. was supported by the Swiss
National Science Foundation (SNSF). Based on observations made with ESO
Telescopes at the La Silla Paranal Observatory under programme ID
60.A-9352(A). The results reported herein benefited from collaborations
and/or information exchange within NASA's Nexus for Exoplanet System
Science (NExSS) research coordination network sponsored by NASA's
Science Mission Directorate.
NR 55
TC 4
Z9 4
U1 3
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 40
DI 10.3847/0004-637X/820/1/40
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000040
ER
PT J
AU Bozza, V
Shvartzvald, Y
Udalski, A
Novati, SC
Bond, IA
Han, C
Hundertmark, M
Poleski, R
Pawlak, M
Szymanski, MK
Skowron, J
Mroz, P
Kozlowski, S
Wyrzykowski, L
Pietrukowicz, P
Soszynski, I
Ulaczyk, K
Beichman, C
Bryden, G
Carey, S
Fausnaugh, M
Gaudi, BS
Gould, A
Henderson, CB
Pogge, RW
Wibking, B
Yee, JC
Zhu, W
Abe, F
Asakura, Y
Barry, RK
Bennett, DP
Bhattacharya, A
Donachie, M
Freeman, M
Fukui, A
Hirao, Y
Inayama, K
Itow, Y
Koshimoto, N
Li, MCA
Ling, CH
Masuda, K
Matsubara, Y
Muraki, Y
Nagakane, M
Nishioka, T
Ohnishi, K
Oyokawa, H
Rattenbury, N
Saito, T
Sharan, A
Sullivan, DJ
Sumi, T
Suzuki, D
Tristram, PJ
Wakiyama, Y
Yonehara, A
Choi, JY
Park, H
Jung, YK
Shin, IG
Albrow, MD
Park, BG
Kim, SL
Lee, CU
Cha, SM
Kim, DJ
Lee, Y
Dominik, M
Jorgensen, UG
Andersen, MI
Bramich, DM
Burgdorf, MJ
Ciceri, S
D'Ago, G
Evans, DF
Jaimes, RF
Gu, SH
Hinse, TC
Kains, N
Kerins, E
Korhonen, H
Kuffmeier, M
Mancini, L
Popovas, A
Rabus, M
Rahvar, S
Rasmussen, RT
Scarpetta, G
Skottfelt, J
Snodgrass, C
Southworth, J
Surdej, J
Unda-Sanzana, E
von Essen, C
Wang, YB
Wertz, O
Maoz, D
Friedmann, M
Kaspi, S
AF Bozza, V.
Shvartzvald, Y.
Udalski, A.
Novati, S. Calchi
Bond, I. A.
Han, C.
Hundertmark, M.
Poleski, R.
Pawlak, M.
Szymanski, M. K.
Skowron, J.
Mroz, P.
Kozlowski, S.
Wyrzykowski, L.
Pietrukowicz, P.
Soszynski, I.
Ulaczyk, K.
Beichman, C.
Bryden, G.
Carey, S.
Fausnaugh, M.
Gaudi, B. S.
Gould, A.
Henderson, C. B.
Pogge, R. W.
Wibking, B.
Yee, J. C.
Zhu, W.
Abe, F.
Asakura, Y.
Barry, R. K.
Bennett, D. P.
Bhattacharya, A.
Donachie, M.
Freeman, M.
Fukui, A.
Hirao, Y.
Inayama, K.
Itow, Y.
Koshimoto, N.
Li, M. C. A.
Ling, C. H.
Masuda, K.
Matsubara, Y.
Muraki, Y.
Nagakane, M.
Nishioka, T.
Ohnishi, K.
Oyokawa, H.
Rattenbury, N.
Saito, To.
Sharan, A.
Sullivan, D. J.
Sumi, T.
Suzuki, D.
Tristram, P. J.
Wakiyama, Y.
Yonehara, A.
Choi, J. -Y.
Park, H.
Jung, Y. K.
Shin, I. -G.
Albrow, M. D.
Park, B. -G.
Kim, S. -L.
Lee, C. -U.
Cha, S. -M.
Kim, D. -J.
Lee, Y.
Dominik, M.
Jorgensen, U. G.
Andersen, M. I.
Bramich, D. M.
Burgdorf, M. J.
Ciceri, S.
D'Ago, G.
Evans, D. F.
Jaimes, R. Figuera
Gu, S. -H.
Hinse, T. C.
Kains, N.
Kerins, E.
Korhonen, H.
Kuffmeier, M.
Mancini, L.
Popovas, A.
Rabus, M.
Rahvar, S.
Rasmussen, R. T.
Scarpetta, G.
Skottfelt, J.
Snodgrass, C.
Southworth, J.
Surdej, J.
Unda-Sanzana, E.
von Essen, C.
Wang, Y. -B.
Wertz, O.
Maoz, D.
Friedmann, M.
Kaspi, S.
CA OGLE Grp
SPITZER Team
MOA Grp
KMTNet Grp
MiNDSTEp
WISE Grp
TI SPITZER OBSERVATIONS OF OGLE-2015-BLG-1212 REVEAL A NEW PATH TOWARD
BREAKING STRONG MICROLENS DEGENERACIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; Galaxy: bulge; gravitational lensing: micro; planets
and satellites: detection; space vehicles
ID GRAVITATIONAL LENSING EXPERIMENT; GALACTIC BULGE; OGLE-III; BINARY;
EVENTS; SATELLITE; PARALLAXES; PHOTOMETRY; SYSTEMS; STARS
AB Spitzer microlensing parallax observations of OGLE-2015-BLG-1212 decisively break. a degeneracy between planetary and binary solutions that is somewhat ambiguous when only ground-based data are considered. Only eight viable models survive out of an initial set of 32 local minima in the parameter space. These models clearly indicate that the lens is a stellar binary system possibly located within the bulge of our Galaxy, ruling out the planetary alternative. We argue that several types of discrete degeneracies can be broken via such space-based parallax observations.
C1 [Bozza, V.; Novati, S. Calchi; D'Ago, G.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo II 132, I-84084 Fisciano, SA, Italy.
[Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Shvartzvald, Y.; Bryden, G.; Henderson, C. B.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Udalski, A.; Poleski, R.; Pawlak, M.; Szymanski, M. K.; Skowron, J.; Mroz, P.; Kozlowski, S.; Wyrzykowski, L.; Pietrukowicz, P.; Soszynski, I.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland.
[Novati, S. Calchi; D'Ago, G.; Scarpetta, G.] IIASS, Via G Pellegrino 19, I-84019 Vietri Sul Mare, SA, Italy.
[Novati, S. Calchi; Beichman, C.] NASA, Exoplanet Sci Inst, CALTECH, MS 100-22, Pasadena, CA 91125 USA.
[Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Private Bag 102-904, Auckland, New Zealand.
[Han, C.; Bhattacharya, A.; Choi, J. -Y.; Park, H.; Jung, Y. K.; Shin, I. -G.] Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea.
[Hundertmark, M.; Jorgensen, U. G.; Korhonen, H.; Kuffmeier, M.; Popovas, A.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Hundertmark, M.; Jorgensen, U. G.; Korhonen, H.; Kuffmeier, M.; Popovas, A.; Skottfelt, J.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Poleski, R.; Fausnaugh, M.; Gaudi, B. S.; Gould, A.; Henderson, C. B.; Pogge, R. W.; Wibking, B.; Zhu, W.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
[Ulaczyk, K.] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England.
[Carey, S.] CALTECH, Ctr Sci, Spitzer, MS 220-6, Pasadena, CA USA.
[Yee, J. C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Abe, F.; Asakura, Y.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Nishioka, T.; Oyokawa, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Barry, R. K.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bennett, D. P.; Suzuki, D.] NASA, Lab Exoplanets & Stellar Astrophys, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bhattacharya, A.; Wakiyama, Y.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Donachie, M.; Freeman, M.; Li, M. C. A.; Rattenbury, N.; Sharan, A.] Univ Auckland, Dept Phys, Private Bag 92019, Auckland, New Zealand.
[Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, 3037-5 Honjo, Asakuchi, Okayama 7190232, Japan.
[Hirao, Y.; Koshimoto, N.; Nagakane, M.; Sumi, T.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Inayama, K.; Yonehara, A.] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan.
[Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand.
[Tristram, P. J.] Mt John Univ Observ, POB 56, Lake Tekapo 8770, New Zealand.
[Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch 8020, New Zealand.
[Cha, S. -M.; Kim, D. -J.; Lee, Y.] Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea.
[Park, B. -G.; Lee, C. -U.; Kim, D. -J.] Korea Astron & Space Sci Inst, Daejon 305348, South Korea.
[Dominik, M.; Jaimes, R. Figuera] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Andersen, M. I.] Univ Copenhagen, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
[Bramich, D. M.] Qatar Fdn, HBKU, QEERI, Doha, Qatar.
[Burgdorf, M. J.] Univ Hamburg, Inst Meteorol, Bundesstr 55, D-20146 Hamburg, Germany.
[Ciceri, S.; Mancini, L.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Evans, D. F.; Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Jaimes, R. Figuera] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Gu, S. -H.; Wang, Y. -B.] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China.
[Kains, N.; Kerins, E.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England.
[Korhonen, H.] Finnish Ctr Astron ESO FINCA, Vaisalantie 20, FI-21500 Piikkio, Finland.
[Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, POB 11155-9161, Tehran, Iran.
[Rasmussen, R. T.; von Essen, C.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
[Skottfelt, J.] Open Univ, Dept Phys Sci, Ctr Elect Imaging, Milton Keynes MK7 6AA, Bucks, England.
[Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England.
[Surdej, J.; Wertz, O.] Inst Astrophys & Geophys, Allee 6 Aout 17,Bat B5c, B-4000 Liege, Belgium.
[Unda-Sanzana, E.] Univ Antofagasta, Fac Ciencias Basicas, Unidad Astronomia, Avda U Antofagasta, Antofagasta 02800, Chile.
[Maoz, D.; Friedmann, M.; Kaspi, S.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
RP Bozza, V (reprint author), Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo II 132, I-84084 Fisciano, SA, Italy.; Bozza, V (reprint author), Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
RI Korhonen, Heidi/E-3065-2016; Hundertmark, Markus/C-6190-2015; D'Ago,
Giuseppe/N-8318-2016; Skowron, Jan/M-5186-2014;
OI Tronsgaard, Rene/0000-0003-1001-0707; Korhonen,
Heidi/0000-0003-0529-1161; Hundertmark, Markus/0000-0003-0961-5231;
D'Ago, Giuseppe/0000-0001-9697-7331; Skowron, Jan/0000-0002-2335-1730;
Dominik, Martin/0000-0002-3202-0343; Wang, Yi-Bo/0000-0002-5172-8558
FU National Science Centre, Poland [MAESTRO 2014/14/A/ST9/00121]; Creative
Research Initiative Program of National Research Foundation of Korea
[2009-0081561]; JPL grant [1500811]; NSF AST [1516842]; NASA through the
Sagan Fellowship Program; JSPS [JSPS23103002, JSPS24253004,
JSPS26247023]; [JSPS25103508]; [JSPS23340064]
FX The OGLE Team thanks Profs. M. Kubiak and G. Pietrzynski, former members
of the OGLE team, for their contribution to the collection of the OGLE
photometric data over the past years. The OGLE project has received
funding from the National Science Centre, Poland, grant MAESTRO
2014/14/A/ST9/00121 to A.U.; Work by C.H. was supported by Creative
Research Initiative Program (2009-0081561) of National Research
Foundation of Korea.; J.C.Y., A.G., and S.C.N. acknowledge support by
JPL grant 1500811. Work by W.Z. and A.G. was supported by NSF AST
1516842.; Work by J.C.Y. was performed under contract with the
California Institute of Technology (Caltech)/Jet Propulsion Laboratory
(JPL) funded by NASA through the Sagan Fellowship Program executed by
the NASA Exoplanet Science Institute.; T.S. acknowledges the financial
support from the JSPS, JSPS23103002, JSPS24253004, and JSPS26247023. The
MOA project is supported by grants JSPS25103508 and JSPS23340064.
NR 40
TC 5
Z9 5
U1 3
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 79
DI 10.3847/0004-637X/820/1/79
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000078
ER
PT J
AU Camilo, F
Reynolds, JE
Ransom, SM
Halpern, JP
Bogdanov, S
Kerr, M
Ray, PS
Cordes, JM
Sarkissian, J
Barr, ED
Ferrara, EC
AF Camilo, F.
Reynolds, J. E.
Ransom, S. M.
Halpern, J. P.
Bogdanov, S.
Kerr, M.
Ray, P. S.
Cordes, J. M.
Sarkissian, J.
Barr, E. D.
Ferrara, E. C.
TI DISCOVERY OF A MILLISECOND PULSAR IN THE 5.4 DAY BINARY 3FGL
J1417.5-4402: OBSERVING THE LATE PHASE OF PULSAR RECYCLING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (PSR J1417-4402)
ID LARGE-AREA TELESCOPE; X-RAY BINARIES; GAMMA-RAY; LOW-MASS; PSR
J1023+0038; NEUTRON-STAR; J1740-5340; COMPANION; NGC-6397; SYSTEM
AB In a search of the unidentified Fermi gamma-ray source 3FGL. J1417.5-4402 with the Parkes radio telescope, we discovered PSR. J1417-4402, a 2.66 ms pulsar having the same 5.4 day orbital period as the optical and X-ray binary identified by Strader et al. The existence of radio pulsations implies that the neutron star is currently not accreting. Substantial outflows from the companion render the radio pulsar undetectable for more than half of the orbit, and may contribute to the observed H alpha emission. Our initial pulsar observations, together with the optically inferred orbit and inclination, imply a mass ratio of 0.171 +/- 0.002, a companion mass of M-2 = 0.33 +/- 0.03 M-circle dot, and a neutron star mass in the range 1.77 <= M-1 <= 2.13 M-circle dot. However, there remains a discrepancy between the distance of 4.4 kpc inferred from the optical properties of the companion and the smaller radio dispersion measure distance of 1.6 kpc. The smaller distance would reduce the inferred Roche-lobe filling factor, increase the inferred inclination angle, and decrease the masses. As a wide binary, PSR. J1417-4402 differs from the radio-eclipsing black widow and redback pulsars being discovered in large numbers by Fermi. It is probably a system that began mass transfer onto the neutron star after the companion star left the main sequence. The companion should end its evolution as a He white dwarf in a 6-20 day orbit, i.e., as a typical binary millisecond pulsar companion.
C1 [Camilo, F.; Halpern, J. P.; Bogdanov, S.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[Camilo, F.] SKA South Africa, ZA-7405 Pinelands, South Africa.
[Reynolds, J. E.; Kerr, M.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Ray, P. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Cordes, J. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Cordes, J. M.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Sarkissian, J.] CSIRO, Parkes Observ, Parkes, NSW 2870, Australia.
[Barr, E. D.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Ferrara, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Camilo, F (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.; Camilo, F (reprint author), SKA South Africa, ZA-7405 Pinelands, South Africa.
OI Ray, Paul/0000-0002-5297-5278
FU Commonwealth of Australia; NASA
FX We are grateful to the ATNF Electronics group led by Warwick Wilson for
their work with the digital filterbanks. We thank Ryan Shannon, Dick
Manchester, and George Hobbs for observing assistance, and Lawrence
Toomey for help with accessing archival data. Phil Edwards accommodated
our stringent observing constraints with grace and efficiency, for which
we are most thankful. We acknowledge stimulating feedback from Thomas
Tauris and Roger Romani. The Parkes Observatory is part of the Australia
Telescope, which is funded by the Commonwealth of Australia for
operation as a National Facility managed by CSIRO. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc. We
acknowledge the use of public data from the Swift data archive. Work by
P. Ray is supported by the NASA Fermi Guest Investigator program.
NR 43
TC 2
Z9 2
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 6
DI 10.3847/0004-637X/820/1/6
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000006
ER
PT J
AU DiSanti, MA
Bonev, BP
Gibb, EL
Paganini, L
Villanueva, GL
Mumma, MJ
Keane, JV
Blake, GA
Dello Russo, N
Meech, KJ
Vervack, RJ
Mckay, AJ
AF DiSanti, M. A.
Bonev, B. P.
Gibb, E. L.
Paganini, L.
Villanueva, G. L.
Mumma, M. J.
Keane, J. V.
Blake, G. A.
Dello Russo, N.
Meech, K. J.
Vervack, R. J., Jr.
McKay, A. J.
TI EN ROUTE TO DESTRUCTION: THE EVOLUTION IN COMPOSITION OF ICES IN COMET
D/2012 S1 (ISON) BETWEEN 1.2 AND 0.34 AU FROM THE SUN AS REVEALED AT
INFRARED WAVELENGTHS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; comets: general; comets: individual (C/2012 S1 (ISON));
molecular processes; Oort Cloud
ID C/2009 P1 GARRADD; NARROW-BAND PHOTOMETRY; C/1996 B2 HYAKUTAKE; KECK II
TELESCOPE; O1 HALE-BOPP; CHEMICAL-COMPOSITION; ECHELLE SPECTROGRAPH;
ORGANIC COMPOSITION; MOLECULAR OBSERVATIONS; PARENT VOLATILES
AB We report production rates for H2O and eight trace molecules (CO, C2H6, CH4, CH3OH, NH3, H2CO, HCN, C2H2) in the dynamically new, Sun-grazing Comet C/2012 S1 (ISON), using high-resolution spectroscopy at Keck II and the NASA IRTF on 10 pre-perihelion dates encompassing heliocentric distances R-h = 1.21-0.34 AU. Measured water production rates spanned two orders of magnitude, consistent with a long-term heliocentric power law Q(H2O) proportional to R-h(-3.1 +/- 0.1). Abundance ratios for CO, C2H6, and CH4 with respect to H2O remained constant with Rh and below their corresponding mean values measured among a dominant sample of Oort Cloud comets. CH3OH was also depleted for R-h > 0.5 AU, but was closer to its mean value for R-h = 0.5 AU. The remaining four molecules exhibited higher abundance ratios within 0.5 AU: for R-h > 0.8 AU, NH3 and C2H2 were consistent with their mean values while H2CO and HCN were depleted. For R-h < 0.5 AU, all four were enriched, with NH3, H2CO, and HCN increasing most. Spatial profiles of gas emission in ISON consistently peaked sunward of the dust continuum, which was asymmetric antisunward and remained singly peaked for all observations. NH3 within 0.5 AU showed a broad spatial distribution, possibly indicating its release in the coma provided that. optical depth effects were unimportant. The column abundance ratio NH2/H2O at 0.83 AU was close to the "typical" NH/OH from optical wavelengths, but was higher within 0.5 AU. Establishing its production rate and testing its parentage (e.g., NH3) require. modeling of coma outflow.
C1 [DiSanti, M. A.; Bonev, B. P.; Gibb, E. L.; Paganini, L.; Villanueva, G. L.; Mumma, M. J.; Blake, G. A.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD USA.
[DiSanti, M. A.; Mumma, M. J.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Code 690, Greenbelt, MD USA.
[Bonev, B. P.; Paganini, L.; Villanueva, G. L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Gibb, E. L.] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA.
[Keane, J. V.; Meech, K. J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Dello Russo, N.; Vervack, R. J., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[McKay, A. J.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
RP DiSanti, MA (reprint author), NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD USA.; DiSanti, MA (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Code 690, Greenbelt, MD USA.
EM michael.a.disanti@nasa.gov
RI Dello Russo, Neil/G-2727-2015; Vervack, Ronald/C-2702-2016
OI Dello Russo, Neil/0000-0002-8379-7304; Vervack,
Ronald/0000-0002-8227-9564
FU NASA Planetary Atmospheres Program [PATM12-0049, NNX12AG60G]; Planetary
Astronomy Program [PAST11-0045]; NSF Astronomy and Astrophysics Program
[AST-1211362, AST-1413736]; National Aeronautics and Space
Administration through the NASA Astrobiology Institute through the
Office of Space Science [08NAI5-0005, NN09DA77A]
FX This work was supported by Research Grant Awards through the NASA
Planetary Atmospheres Program (PATM12-0049 to M.A.D., and NNX12AG60G to
B.P.B.), Planetary Astronomy Program (PAST11-0045 to M.J.M.), and the
NSF Astronomy and Astrophysics Program (AST-1211362 to B.P.B. and
E.L.G., and AST-1413736 to J.V.K.). This material is based in part on
work supported by the National Aeronautics and Space Administration
through the NASA Astrobiology Institute, issued through the Office of
Space Science under grant 08NAI5-0005 to M.J.M., and under Cooperative
Agreement Number NN09DA77A to K.J.M. We thank the Keck and IRTF for
providing dedicated observing time for Comet ISON, and J. Green, K.
Fast, and L. Johnson in the Planetary Science Division at NASA-HQ for
their encouragement in supporting the overall ground-and space-based
ISON observing campaign. We thank an anonymous referee for comments that
improved the mauscript. M.A.D. gratefully acknowledges Strategic Science
support from the Solar System Exploration Division at NASA-GSFC for his
participation as a member of the Comet ISON Observing Campaign team.
B.P.B.'s contribution to the Comet ISON Observing Campaign is dedicated
to the memory of Hristo Hristov for his long distinguished service as a
physics teacher in The Foreign Language School "Romain Rolland," Stara
Zagora, Bulgaria. We recognize the very significant cultural role and
reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community and feel most fortunate to conduct these
observations from this mountain.
NR 69
TC 2
Z9 2
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 34
DI 10.3847/0004-637X/820/1/34
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000034
ER
PT J
AU Guidoni, SE
DeVore, CR
Karpen, JT
Lynch, BJ
AF Guidoni, S. E.
DeVore, C. R.
Karpen, J. T.
Lynch, B. J.
TI MAGNETIC-ISLAND CONTRACTION AND PARTICLE ACCELERATION IN SIMULATED
ERUPTIVE SOLAR FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; magnetic reconnection; Sun: coronal mass
ejections (CMEs); Sun: flares
ID HARD X-RAY; QUASI-PERIODIC PULSATIONS; CORONAL MASS EJECTIONS; CURRENT
SHEET; ELECTRON ACCELERATION; NUMERICAL EXPERIMENTS; ENERGETIC
PARTICLES; RECONNECTION; MODEL; RADIO
AB The mechanism that accelerates particles to the energies required to produce the observed high-energy impulsive emission in solar flares is not well understood. Drake et al. proposed a mechanism for accelerating electrons in contracting magnetic islands formed by kinetic reconnection in multi-layered current sheets (CSs). We apply these ideas to sunward-moving flux ropes (2.5D magnetic islands) formed during fast reconnection in a simulated eruptive flare. A simple analytic model is used to calculate the energy gain of particles orbiting the field lines of the contracting magnetic islands in our ultrahigh-resolution 2.5D numerical simulation. We find that the estimated energy gains in a single island range up to a factor of five. This is higher than that found by Drake et al. for islands in the terrestrial magnetosphere and at the heliopause, due to strong plasma compression that occurs at the flare CS. In order to increase their energy by two orders of magnitude and plausibly account for the observed high-energy flare emission, the electrons must visit multiple contracting islands. This mechanism should produce sporadic emission because island formation is intermittent. Moreover, a large number of particles could be accelerated in each magnetohydrodynamic-scale island, which may explain the inferred rates of energetic-electron production in flares. We conclude that island contraction in the flare CS is a promising candidate for electron acceleration in solar eruptions.
C1 [Guidoni, S. E.] Catholic Univ Amer, 620 Michigan Ave Northeast, Washington, DC 20064 USA.
[Guidoni, S. E.; DeVore, C. R.; Karpen, J. T.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Lynch, B. J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Guidoni, SE (reprint author), Catholic Univ Amer, 620 Michigan Ave Northeast, Washington, DC 20064 USA.
EM silvina.e.guidoni@nasa.gov
RI Lynch, Benjamin/B-1300-2013;
OI Lynch, Benjamin/0000-0001-6886-855X
FU NASA Heliophysics Supporting Research program
FX We thank Prof. Jim Drake, Dr. Spiro Antiochos, and Dr. Peter Wyper for
helpful comments and advice. This research was supported in part by the
NASA Heliophysics Supporting Research program. Resources supporting this
work were provided by the NASA High-End Computing Program through the
NASA Center for Climate Simulation at Goddard Space Flight Center.
NR 109
TC 5
Z9 5
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 60
DI 10.3847/0004-637X/820/1/60
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000059
ER
PT J
AU Houde, M
Hull, CLH
Plambeck, RL
Vaillancourt, JE
Hildebrand, RH
AF Houde, Martin
Hull, Charles L. H.
Plambeck, Richard L.
Vaillancourt, John E.
Hildebrand, Roger H.
TI DISPERSION OF MAGNETIC FIELDS IN MOLECULAR CLOUDS. IV. ANALYSIS OF
INTERFEROMETRY DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: magnetic fields; polarization; turbulence
ID AMBIPOLAR DIFFUSION SCALE; ION SPECTRA; POLARIZATION; POLARIMETRY;
TURBULENCE; REGIONS; DUST; CORE; M51
AB We expand on the dispersion analysis of polarimetry maps toward applications to interferometry data. We show how the filtering of low spatial frequencies can be accounted for within the idealized Gaussian turbulence model, initially introduced for single-dish data analysis, to recover reliable estimates for correlation lengths of magnetized turbulence, as well as magnetic field strengths (plane-of-the-sky component) using the Davis-Chandrasekhar-Fermi method. We apply our updated technique to TADPOL/CARMA data obtained on W3(OH), W3 Main, and DR21(OH). For W3(OH), our analysis yields a turbulence correlation length delta similar or equal to 19 mpc, a ratio of turbulent-to-total magnetic energy < B-t(2)> / < B-2 > similar or equal to 0.58 and a magnetic field strength B-0 similar to 1.1 mG; for W3 Main delta similar or equal to 22 mpc, < B-t(2)> / < B-2 > similar or equal to 0.74 and B similar to 0.7 mG; while for DR21(OH) delta similar or equal to 12 mpc, < B-t(2)> / < B-2 > similar or equal to 0.70 and B-0 similar or equal to 1.2 mG.
C1 [Houde, Martin] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Houde, Martin] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Hull, Charles L. H.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Plambeck, Richard L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Plambeck, Richard L.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA.
[Vaillancourt, John E.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hildebrand, Roger H.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Hildebrand, Roger H.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Hildebrand, Roger H.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
RP Houde, M (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.; Houde, M (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
FU NSERC Discovery Grant; Canada Research Chair; Canada Foundation for
Innovation; Ontario Innovation Trust; Western's Academic Development
Fund programs; National Science Foundation; CARMA partner universities
FX M.H.'s research is funded through the NSERC Discovery Grant, Canada
Research Chair, Canada Foundation for Innovation, Ontario Innovation
Trust, and Western's Academic Development Fund programs. CARMA
development and operations were funded by the National Science
Foundation and the CARMA partner universities.
NR 36
TC 4
Z9 4
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 38
DI 10.3847/0004-637X/820/1/38
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000038
ER
PT J
AU Jontof-Hutter, D
Ford, EB
Rowe, JF
Lissauer, JJ
Fabrycky, DC
Van Laerhoven, C
Agol, E
Deck, KM
Holczer, T
Mazeh, T
AF Jontof-Hutter, Daniel
Ford, Eric B.
Rowe, Jason F.
Lissauer, Jack J.
Fabrycky, Daniel C.
Van Laerhoven, Christa
Agol, Eric
Deck, Katherine M.
Holczer, Tomer
Mazeh, Tsevi
TI SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS
BETWEEN 3 AND 8M(circle plus) WITH DIVERSE DENSITIES AND INCIDENT FLUXES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: individual (Kepler-60, Kepler-177, Kepler-26, Kepler-29,
Kepler-307); techniques: photometric
ID MULTIPLE-PLANET SYSTEMS; CHAIN MONTE-CARLO; EXTRASOLAR PLANETS;
LIGHT-CURVE; DIFFERENTIAL EVOLUTION; TERRESTRIAL PLANETS; ROCKY PLANET;
HOT NEPTUNE; HARPS-N; M DWARF
AB We infer dynamical masses in eight multiplanet systems using transit times measured from Kepler's complete data. set, including short-cadence data where available. Of the 18 dynamical masses that we infer, 10 pass multiple tests for robustness. These are in systems. Kepler-26 (KOI-250), Kepler-29 (KOI-738), Kepler-60 (KOI-2086), Kepler-105 (KOI-115), and Kepler-307 (KOI-1576). Kepler-105 c has a radius of 1.3 R-circle plus and a density consistent with an Earth-like composition. Strong transit timing variation (TTV) signals were detected from additional planets, but their inferred masses were sensitive to outliers or consistent solutions could not be found with independently measured transit times, including planets orbiting. Kepler-49 (KOI-248), Kepler-57 (KOI-1270), Kepler-105 (KOI-115), and Kepler-177 (KOI-523). Nonetheless, strong upper limits on the mass of Kepler-177 c imply an extremely low density of. similar to 0.1 g cm(-3). In most cases, individual orbital eccentricities were poorly constrained owing. to degeneracies in TTV inversion. For five planet pairs in our sample, strong secular interactions imply a moderate. to. high likelihood of apsidal alignment over a wide range of possible eccentricities. We also find solutions for the three planets known to orbit Kepler-60 in a Laplace-like resonance chain. However, nonlibrating solutions also match the transit. timing data. For six systems, we calculate more precise stellar parameters than previously known, enabling useful constraints on planetary densities where we have secure mass measurements. Placing these exoplanets on the mass-radius diagram, we find that. a wide range of densities is. observed among sub-Neptune-mass planets and that the range in observed densities is anticorrelated with incident flux.
C1 [Jontof-Hutter, Daniel; Ford, Eric B.] Penn State Univ, Dept Astron, University Pk, PA 16802 USA.
[Rowe, Jason F.] Univ Montreal, Dept Phys, Montreal, PQ H3T 1J4, Canada.
[Lissauer, Jack J.] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.
[Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Van Laerhoven, Christa] Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Deck, Katherine M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Holczer, Tomer; Mazeh, Tsevi] Tel Aviv Univ, Sch Phys & Astron, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Tel Aviv, Israel.
RP Jontof-Hutter, D (reprint author), Penn State Univ, Dept Astron, University Pk, PA 16802 USA.
EM dxj14@psu.edu
FU NASA Exoplanets Research Program [NNX15AE21G]; NASA's Science Mission
Directorate; Center for Exoplanets and Habitable Worlds; Pennsylvania
State University; Eberly College of Science; Pennsylvania Space Grant
Consortium; NASA [NNX13AF20G, NNX13AF62G]; NASA Astrobiology Institutes
Virtual Planetary Laboratory - NASA [NNH05ZDA001C]; Joint Center for
Planetary Astronomy fellowship at Caltech
FX We wish to thank our anonymous referee for a helpful review that
improved this paper. D.J., E.F., and J.L. acknowledge support from NASA
Exoplanets Research Program award #NNX15AE21G. The results reported
herein benefitted from collaborations and/or information exchange within
NASA's Nexus for Exoplanet System Science (NExSS) research coordination
network sponsored by NASA's Science Mission Directorate. D.J. and E.F.
gratefully acknowledge that this work was partially supported by funding
from the Center for Exoplanets and Habitable Worlds. The Center for
Exoplanets and Habitable Worlds is supported by the Pennsylvania State
University, the Eberly College of Science, and the Pennsylvania Space
Grant Consortium. E.A. acknowledges support from NASA grants NNX13AF20G,
NNX13AF62G, and NASA Astrobiology Institutes Virtual Planetary
Laboratory, supported by NASA under cooperative agreement NNH05ZDA001C.
K.D. acknowledges support from the Joint Center for Planetary Astronomy
fellowship at Caltech.
NR 89
TC 11
Z9 11
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 39
DI 10.3847/0004-637X/820/1/39
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000039
ER
PT J
AU Kohn, SA
Shkolnik, EL
Weinberger, AJ
Carlberg, JK
Llama, J
AF Kohn, Saul A.
Shkolnik, Evgenya L.
Weinberger, Alycia J.
Carlberg, Joleen K.
Llama, Joe
TI SEARCHING FOR SPECTROSCOPIC BINARIES WITHIN TRANSITION DISK OBJECTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: spectroscopic; circumstellar matter; stars: pre-main sequence
ID LOW-MASS STARS; T-TAURI STARS; PRE-MAIN-SEQUENCE; ALL-SKY SURVEY;
RHO-OPHIUCHI CLOUD; SPITZER C2D SURVEY; SOLAR-TYPE STARS; ANGULAR
RESOLUTION MEASUREMENTS; OBSERVED LUMINOSITY SPREAD; YOUNG BROWN DWARFS
AB Transition disks (TDs) are intermediate stage circumstellar disks characterized by an inner gap within the disk structure. To test whether these gaps may have been formed by closely orbiting, previously undetected stellar companions, we collected high-resolution optical spectra of 31 TD objects to search for spectroscopic binaries (SBs). Twenty-four of these objects are in Ophiuchus and seven are within the Coronet, Corona Australis, and Chameleon I star-forming regions. We measured radial velocities for multiple epochs, obtaining a median precision of 400 ms(-1). We identified double-lined SB SSTc2d J163154.7-250324 in Ophiuchus, which we determined to be composed of a K7(+/- 0.5) and a K9(+/- 0.5) star, with orbital limits of a < 0.6 au and P < 150 days. This results in an SB fraction of 0.04(-0.03+)(0.12) in Ophiuchus, which is consistent with other spectroscopic surveys of non-TD objects in the region. This similarity suggests that TDs are not preferentially sculpted by the presence of close binaries and that planet formation around close binaries may take place over similar timescales to that around single stars.
C1 [Kohn, Saul A.; Shkolnik, Evgenya L.; Llama, Joe] Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA.
[Kohn, Saul A.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Shkolnik, Evgenya L.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Weinberger, Alycia J.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd,NW, Washington, DC 20015 USA.
[Carlberg, Joleen K.] NASA, GSFC Code 667, Greenbelt, MD 20771 USA.
[Llama, Joe] Sch Phys & Astron, SUPA, North Haugh, St Andrews KY16 9SS, Fife, Scotland.
RP Kohn, SA (reprint author), Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA.; Kohn, SA (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
EM saulkohn@sas.upenn.edu
OI Kohn, Saul/0000-0001-6744-5328; Weinberger, Alycia/0000-0001-6654-7859
FU NSF REU grant through Northern Arizona University [AST-1004107]; Lowell
Observatory; NASA Origins of the Solar System grant [NNX13AH79G]; STFC
grant [ST/M001296/1]
FX We thank M. Hughes for her contribution of RX J1852.3-3700 to the target
list prior to its publication; L. Prato, C. Johns-Krull, and Cullen H.
Blake for helpful discussions; and the anonymous referee for her/his
insightful comments. S. A. Kohn acknowledges the support of NSF REU
grant AST-1004107 through Northern Arizona University and Lowell
Observatory. J. Llama acknowledges support from NASA Origins of the
Solar System grant No. NNX13AH79G and from STFC grant ST/M001296/1. This
research made use of the SIMBAD database, operated at CDS, Strasbourg,
France.
NR 136
TC 1
Z9 1
U1 1
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 2
DI 10.3847/0004-637X/820/1/2
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000002
ER
PT J
AU LaMassa, SM
Ricarte, A
Glikman, E
Urry, CM
Stern, D
Yaqoob, T
Lansbury, GB
Civano, F
Boggs, SE
Brandt, WN
Chen, CTJ
Christensen, FE
Craig, WW
Hailey, CJ
Harrison, F
Hickox, RC
Koss, M
Ricci, C
Treister, E
Zhang, W
AF LaMassa, Stephanie M.
Ricarte, Angelo
Glikman, Eilat
Urry, C. Megan
Stern, Daniel
Yaqoob, Tahir
Lansbury, George B.
Civano, Francesca
Boggs, Steve E.
Brandt, W. N.
Chen, Chien-Ting J.
Christensen, Finn E.
Craig, William W.
Hailey, Chuck J.
Harrison, Fiona
Hickox, Ryan C.
Koss, Michael
Ricci, Claudio
Treister, Ezequiel
Zhang, Will
TI PEERING THROUGH THE DUST: NuSTAR OBSERVATIONS OF TWO FIRST-2MASS RED
QUASARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; infrared: galaxies; quasars: individual (F2M
0380+3759, F2M 1227+3214); X-rays: individual (F2M 0830+3759, F2M
1227+3214)
ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; XMM-NEWTON
OBSERVATIONS; DIGITAL SKY SURVEY; RAY SPECTRAL MODEL; WIDE-FIELD SURVEY;
X-RAY; REDDENED QUASARS; COSMOS FIELD; SEYFERT-GALAXIES
AB Some reddened quasars appear to be transitional objects in the paradigm of merger-induced black hole growth/galaxy evolution, where a heavily obscured nucleus starts to be unveiled by powerful quasar winds evacuating the surrounding cocoon of dust and gas. Hard X-ray observations are able to peer through this gas and dust, revealing the properties of circumnuclear obscuration. Here, we present NuSTAR and XMM-Newton/Chandra observations of FIRST-2MASS-selected red quasars F2M 0830+3759 and F2M 1227+3214. We find that though F2M 0830 +3759 is moderately obscured (N-H,(Z) = (2.1 +/- 0.2) x 10(22) cm(-2)) and F2M 1227+3214 is mildly absorbed (N-H,(Z) = 3.4(- 0.7)(+0.8) x 10(21) cm(-2)) along the line of sight, heavier global obscuration may be present in both sources, with N-H,(S) = 3.7(- 2.6)(+4.1) x 10(23) cm(-2) and <5.5 x 10(23) cm(-2) for F2M 0830+3759 and F2M 1227+3214, respectively. F2M 0830+3759 also has an excess of soft X-ray emission below 1 keV, which is well accommodated by a model where 7% of the intrinsic X-ray emission from the active galactic nucleus (AGN) is scattered into the line of sight. While F2M 1227+3214 has a dust-to-gas ratio (E(B - V)/N-H) consistent with the Galactic value, the value of E(B - V)/N-H for F2M 0830+3759 is lower than the Galactic standard, consistent with the paradigm that the dust resides on galactic scales while the X-ray reprocessing gas originates within the dust sublimation zone of the broad-line region. The X-ray and 6.1 mu m luminosities of these red quasars are consistent with the empirical relations derived for high-luminosity, unobscured quasars, extending the parameter space of obscured AGNs previously observed by NuSTAR to higher luminosities.
C1 [LaMassa, Stephanie M.; Urry, C. Megan; Civano, Francesca] Yale Ctr Astron & Astrophys, Dept Phys, POB 208120, New Haven, CT 06520 USA.
[LaMassa, Stephanie M.; Urry, C. Megan; Civano, Francesca] Yale Univ, Dept Phys, POB 208121, New Haven, CT 06520 USA.
[LaMassa, Stephanie M.; Zhang, Will] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ricarte, Angelo] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Glikman, Eilat] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-221, Pasadena, CA 91109 USA.
[Yaqoob, Tahir] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Lansbury, George B.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
[Civano, Francesca; Hickox, Ryan C.] Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA.
[Civano, Francesca] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Boggs, Steve E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Brandt, W. N.; Chen, Chien-Ting J.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Brandt, W. N.; Chen, Chien-Ting J.] Penn State Univ, Inst Gravitat & Cosmos, 525 Davey Lab, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Dept Phys, 525 Davey Lab, University Pk, PA 16802 USA.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, Chuck J.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[Harrison, Fiona] CALTECH, Cahill Ctr Astron & Astrophys, 1216 E Calif Blvd, Pasadena, CA 91125 USA.
[Koss, Michael] ETH, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Ricci, Claudio] Pontificia Univ Catolica Chile, Inst Astrofis, Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Treister, Ezequiel] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile.
RP LaMassa, SM (reprint author), Yale Ctr Astron & Astrophys, Dept Phys, POB 208120, New Haven, CT 06520 USA.
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Urry, Meg/0000-0002-0745-9792
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; Gruber
Science Fellowship; Cottrell College Award through the Research
Corporation for Science Advancement; Caltech NuSTAR subcontract
[44A-1092750]; NASA ADP grant [NNX10AC99G]; NASA through ADAP award
[NNX12AE38G]; National Science Foundation [1211096, 1515364]; Sloan
Research Fellowship; Dartmouth Class of Faculty Fellowship;
CONICYT-Chile grants ["EMBIGGEN" Anillo ACT1101, FONDECYT 1141218,
Basal-CATA PFB-06/2007]
FX We thank the referee for a careful reading of this manuscript and
helpful comments. This work was supported under NASA contract No.
NNG08FD60C, and made use of data from the NuSTAR mission, a project led
by the California Institute of Technology, managed by the Jet Propulsion
Laboratory, and funded by the National Aeronautics and Space
Administration. We thank the NuSTAR Operations, Software and Calibration
teams for support with the execution and analysis of these observations.
This research has made use of the NuSTAR Data Analysis Software
(NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC,
Italy) and the California Institute of Technology (USA). AR is supported
by the Gruber Science Fellowship. EG acknowledges the generous support
of the Cottrell College Award through the Research Corporation for
Science Advancement. WNB acknowledges support from Caltech NuSTAR
subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. RCH acknowledges
support from NASA through ADAP award NNX12AE38G, the National Science
Foundation through grant nos. 1211096 and 1515364, a Sloan Research
Fellowship, and a Dartmouth Class of 1962 Faculty Fellowship. CR
acknowledges financial support from the CONICYT-Chile grants "EMBIGGEN"
Anillo ACT1101, FONDECYT 1141218, Basal-CATA PFB-06/2007.
NR 108
TC 3
Z9 3
U1 2
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 70
DI 10.3847/0004-637X/820/1/70
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000069
ER
PT J
AU Line, MR
Parmentier, V
AF Line, Michael R.
Parmentier, Vivien
TI THE INFLUENCE OF NONUNIFORM CLOUD COVER ON TRANSIT TRANSMISSION SPECTRA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: analytical; planets and satellites: atmospheres; planets and
satellites: composition; planets and satellites: individual (HD.
189733b, HAT-P-11b)
ID HUBBLE-SPACE-TELESCOPE; HOT JUPITER WASP-43B; PLANET HD 189733B; BROWN
DWARFS; SUPER-EARTHS; ATMOSPHERIC CIRCULATION; PHASE CURVES; GJ 1214B;
EXOPLANET ATMOSPHERE; 3-DIMENSIONAL MODELS
AB We model the impact of nonuniform cloud cover on transit transmission spectra. Patchy clouds exist in nearly every solar system atmosphere, brown dwarfs, and transiting exoplanets. Our major findings suggest that fractional cloud coverage can exactly mimic high mean molecular weight atmospheres and vice. versa over certain wavelength regions, in particular, over the Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) bandpass (1.1-1.7 mu m). We also find that patchy cloud coverage exhibits a signature that is different from uniform global clouds. Furthermore, we explain analytically why the "patchy cloud-high mean molecular weight" degeneracy exists. We also explore the degeneracy of nonuniform cloud coverage in atmospheric retrievals on both synthetic and real planets. We find from retrievals on a synthetic solar composition hot Jupiter with patchy clouds and a cloud-free high mean molecular weight warm Neptune. that both cloud-free high mean molecular weight atmospheres and partially cloudy atmospheres can explain the data equally well. Another key finding is that the HST WFC3 transit transmission spectra of two well-observed objects, the hot Jupiter HD. 189733b and the warm Neptune HAT-P-11b, can be explained well by solar composition atmospheres with patchy clouds without the need to invoke high mean molecular weight or global clouds. The degeneracy between high molecular weight and solar composition partially cloudy atmospheres can be broken by observing the molecular Rayleigh scattering differences between the two. Furthermore, the signature of partially cloudy limbs also appears as a similar to 100 ppm residual in the ingress and egress of the transit light curves, provided. that the transit timing is known to seconds.
C1 [Line, Michael R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Line, Michael R.] Bay Area Environm Res Inst, 625 2nd St Ste 209, Petaluma, CA 94952 USA.
[Line, Michael R.] Arizona State Univ, Sch Earth & Space Explorat, 781 S Terrace Rd, Tempe, AZ 85281 USA.
[Line, Michael R.; Parmentier, Vivien] Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA.
RP Line, MR (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.; Line, MR (reprint author), Bay Area Environm Res Inst, 625 2nd St Ste 209, Petaluma, CA 94952 USA.; Line, MR (reprint author), Arizona State Univ, Sch Earth & Space Explorat, 781 S Terrace Rd, Tempe, AZ 85281 USA.; Line, MR (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA.
EM mrline@ucsc.edu
FU NASA through Hubble Fellowship - Space Telescope Science Institute
[51362]; NASA [NAS 5-26555]; Sagan Postdoctoral Fellowship through the
NASA Exoplanet Science Institute; National Science Foundation
[AST-1229745]; University of California, Santa Cruz
FX We thank Jonathan Fortney and Mark Swain for reading the manuscript and
providing useful comments,. and Daniel Thorngren, Leslie Rogers, and
Caroline Morley for useful discussions. M.R.L. acknowledges support
provided by NASA through Hubble Fellowship grant 51362 awarded by the
Space Telescope Science Institute, which is operated by the Association
of Universities for Research in Astronomy, Inc., for NASA, under the
contract NAS 5-26555. V.P. acknowledges support from the Sagan
Postdoctoral Fellowship through the NASA Exoplanet Science Institute.
The simulations for this research were carried out on the UCSC Hyades
computing cluster, which is supported by National Science Foundation
(award number AST-1229745) and University of California, Santa Cruz.
NR 69
TC 10
Z9 10
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 78
DI 10.3847/0004-637X/820/1/78
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000077
ER
PT J
AU Maltseva, E
Petrignani, A
Candian, A
Mackie, CJ
Huang, XC
Lee, TJ
Tielens, AGGM
Oomens, J
Buma, WJ
AF Maltseva, Elena
Petrignani, Annemieke
Candian, Alessandra
Mackie, Cameron J.
Huang, Xinchuan
Lee, Timothy J.
Tielens, Alexander G. G. M.
Oomens, Jos
Buma, Wybren Jan
TI HIGH-RESOLUTION IR ABSORPTION SPECTROSCOPY OF POLYCYCLIC AROMATIC
HYDROCARBONS: THE REALM OF ANHARMONICITY (vol 814, 23, 2015)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Maltseva, Elena; Buma, Wybren Jan] Univ Amsterdam, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Petrignani, Annemieke; Candian, Alessandra; Mackie, Cameron J.; Tielens, Alexander G. G. M.] Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
[Petrignani, Annemieke; Oomens, Jos] Radboud Univ Nijmegen, Toernooiveld 7, NL-6525 ED Nijmegen, Netherlands.
[Huang, Xinchuan] SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA.
[Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Buma, WJ (reprint author), Univ Amsterdam, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.; Petrignani, A (reprint author), Radboud Univ Nijmegen, Toernooiveld 7, NL-6525 ED Nijmegen, Netherlands.
EM petrignani@strw.leidenuniv.nl; w.j.buma@uva.nl
RI HUANG, XINCHUAN/A-3266-2013; Lee, Timothy/K-2838-2012; Buma, Wybren
Jan/F-6691-2011
OI Buma, Wybren Jan/0000-0002-1265-8016
NR 1
TC 0
Z9 0
U1 3
U2 14
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 81
DI 10.3847/0004-637X/820/1/81
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000080
ER
PT J
AU Man, AWS
Greve, TR
Toft, S
Magnelli, B
Karim, A
Ilbert, O
Salvato, M
Le Floc'h, E
Bertoldi, F
Casey, CM
Lee, N
Li, YX
Navarrete, F
Sheth, K
Smolcic, V
Sanders, DB
Schinnerer, E
Zirm, AW
AF Man, Allison W. S.
Greve, Thomas R.
Toft, Sune
Magnelli, Benjamin
Karim, Alexander
Ilbert, Olivier
Salvato, Mara
Le Floc'h, Emeric
Bertoldi, Frank
Casey, Caitlin M.
Lee, Nicholas
Li, Yanxia
Navarrete, Felipe
Sheth, Kartik
Smolcic, Vernesa
Sanders, David B.
Schinnerer, Eva
Zirm, Andrew W.
TI CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z=3: A
STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: ISM; galaxies:
star formation; galaxies: statistics; infrared: ISM
ID ACTIVE GALACTIC NUCLEI; STAR-FORMATION RATES; SIMILAR-TO 2; COSMOS
FIELD; FORMING GALAXIES; AGN POPULATION; EVOLUTION; HERSCHEL; MASS;
FEEDBACK
AB We performed a comprehensive stacking analysis on similar to 14,200 quiescent galaxy (QG) candidates at z = 0-3 across mid-, far-infrared (MIR and FIR), and radio wavelengths. Identified via their rest-frame NUV - r and r - J colors, the QG candidates (M-* = 10(9.8-12.2) M-circle dot) have drastically different IR and radio properties depending on their 24 mu m emission strength. The fraction of QG candidates with strong 24 mu m emission (equivalent to inferred star formation rates SFR24 >= 100 M-circle dot yr(-1), hereafter "IR-bright") increases with redshift and peaks at 15%, and their stacked MIPS 24 mu m, Herschel (PACS and SPIRE) and VLA emissions are consistent with being star-forming galaxies (SFGs). In contrast, the majority of QG candidates are faint or undetected at 24 mu m individually (i.e., SFR24 < 100 M-circle dot yr(-1), hereafter "IR-faint"). Their low dust-obscured SFRs derived from Herschel stacking (SFRH less than or similar to 3, 15, 50 M-circle dot yr(-1) out to z similar to 1, 2, 3) are > 2.5-12.5x lower than compared to SFGs. This is consistent with the quiescence, as expected from their low unobscured SFRs, as inferred from modeling their ultraviolet-to-NIR photometry. The discrepancy between the L-IR derived from stacking Herschel and 24 mu m indicates that IR-faint QGs have dust SEDs that are different from those of SFGs. For the most massive (M-star >= 10(11) M-circle dot) IR-faint QGs at z < 1.5, the stacked 1.4 GHz emission is in excess of that expected from other SFR indicators, suggesting a widespread presence of low-luminosity active galactic nuclei. Our results reaffirm the existence of a significant population of QGs out to z. =. 3, thus corroborating the need to quench star formation in galaxies at early epochs.
C1 [Man, Allison W. S.; Toft, Sune; Lee, Nicholas; Zirm, Andrew W.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-1168 Copenhagen, Denmark.
[Man, Allison W. S.; Lee, Nicholas; Li, Yanxia; Sanders, David B.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Man, Allison W. S.] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Greve, Thomas R.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
[Magnelli, Benjamin; Karim, Alexander; Bertoldi, Frank; Navarrete, Felipe] Univ Bonn, Argelander Inst Astron, Auf Hugel 71, D-53121 Bonn, Germany.
[Ilbert, Olivier] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France.
[Salvato, Mara] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Le Floc'h, Emeric] Univ Paris Diderot, CEA, CNRS, DSM,IRFU,Lab AIM, F-91190 Gif, France.
[Casey, Caitlin M.] Univ Texas Austin, Dept Astron, 2515 Speedway Stop C1400, Austin, TX 78712 USA.
[Sheth, Kartik] NASA Headquarters, Sci Miss Directorate, Washington, DC 20546 USA.
[Smolcic, Vernesa] Univ Zagreb, Dept Phys, Bijenicka Cesta 32, Zagreb 10002, Croatia.
[Schinnerer, Eva] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
RP Man, AWS (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-1168 Copenhagen, Denmark.; Man, AWS (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.; Man, AWS (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM allison.man@eso.org
OI Casey, Caitlin/0000-0002-0930-6466; Schinnerer, Eva/0000-0002-3933-7677
FU Dark Cosmology Centre - DNRF; STFC; ERC [648179]; Collaborative Research
Council 956 - Deutsche Forschungsgemeinschaft (DFG); DFG priority
program 1573 "The physics of the interstellar medium"; McCue Fellowship
through the University of California, Irvine's Center for Cosmology;
European Union's Seventh Frame-work program (ERC Starting Grant,
"CoSMass") [337595]; Instrument Centre for Danish Astrophysics (IDA);
ESO Telescopes at the La Silla Paranal Observatory [179.A-2005]
FX We thank the COSMOS, UltraVISTA, PEP, and HerMES collaborations for
providing the data used in this work. We are grateful to the anonymous
referee for the invaluable comments that improved this manuscript. A.M.
thanks Anna Gallazzi, Mark Sargent, Ryan Quadri, Brian Lemaux, and Julie
Wardlow for helpful discussions. A.M. acknowledges the support of the
Dark Cosmology Centre, which is funded by DNRF. T.R.G. acknowledges
support from an STFC Advanced Fellowship. S.T. acknowledges support from
the ERC Consolidator Grant funding scheme (project ConTExt, grant number
648179). A.K. acknowledges support by the Collaborative Research Council
956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft
(DFG). Support for B.M. was provided by the DFG priority program 1573
"The physics of the interstellar medium". C.M.C. acknowledges support
from a McCue Fellowship through the University of California, Irvine's
Center for Cosmology. V.S. is funded by the European Union's Seventh
Frame-work program under grant agreement 337595 (ERC Starting Grant,
"CoSMass"). A.Z. acknowledges support by the Instrument Centre for
Danish Astrophysics (IDA). This work is based on data products from
observations made with ESO Telescopes at the La Silla Paranal
Observatory under ESO program ID 179.A-2005 and on data products
produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of
the UltraVISTA consortium.
NR 60
TC 3
Z9 3
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 11
DI 10.3847/0004-637X/820/1/11
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000011
ER
PT J
AU Racine, B
Jewell, JB
Eriksen, HK
Wehus, IK
AF Racine, B.
Jewell, J. B.
Eriksen, H. K.
Wehus, I. K.
TI COSMOLOGICAL PARAMETERS FROM CMB MAPS WITHOUT LIKELIHOOD APPROXIMATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmological parameters; cosmology:
observations; methods: numerical
ID MICROWAVE BACKGROUND DATA; POWER SPECTRUM ESTIMATION; BAYESIAN-ANALYSIS;
INFERENCE
AB We propose an efficient Bayesian Markov chain Monte Carlo (MCMC) algorithm for estimating cosmological parameters from cosmic microwave background (CMB) data without the use of likelihood approximations. It builds on a previously developed Gibbs sampling framework that allows for exploration of the joint CMB sky signal and power spectrum posterior, P(s, C-l vertical bar d), and addresses a long-standing problem of efficient parameter estimation simultaneously in regimes of high and low signal-to-noise ratio. To achieve this, our new algorithm introduces a joint Markov chain move in which both the signal map and power spectrum are synchronously modified, by rescaling the map according to the proposed power spectrum before evaluating the Metropolis-Hastings accept probability. Such a move was already introduced by Jewell et al., who used it to explore low signal-to-noise posteriors. However, they also found that the same algorithm is inefficient in the high signal-tonoise regime, since a brute-force rescaling operation does not account for phase information. This problem is mitigated in the new algorithm by subtracting the Wiener filter mean field from the proposed map prior to rescaling, leaving high signal-to-noise information invariant in the joint step, and effectively only rescaling the low signal-to-noise component. To explore the full posterior, the new joint move is then interleaved with a standard conditional Gibbs move for the sky map. We apply our new algorithm to simplified simulations for which we can evaluate the exact posterior to study both its accuracy and its performance, and find good agreement with the exact posterior; marginal means agree to less than or similar to 0.006 sigma and standard deviations to better than similar to 3%. The Markov chain correlation length is of the same order of magnitude as those obtained by other standard samplers in the field.
C1 [Racine, B.; Eriksen, H. K.; Wehus, I. K.] Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway.
[Jewell, J. B.; Wehus, I. K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Racine, B (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway.
EM benjamin.racine@astro.uio.no
FU Research Council of Norway; ERC [StG2010-257080]
FX B.R. and H.K.E. thank Charles Lawrence and the Jet Propulsion Laboratory
(JPL) for their hospitality during summer 2015, where this project was
initiated. We acknowledge the use of the CAMB and HEALPix (Gorski et al.
2005) software packages. B.R. acknowledges funding from the Research
Council of Norway. This project was supported by the ERC Starting Grant
StG2010-257080. Part of the research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA.
NR 22
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 31
DI 10.3847/0004-637X/820/1/31
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000031
ER
PT J
AU Ricci, C
Bauer, FE
Arevalo, P
Boggs, S
Brandt, WN
Christensen, FE
Craig, WW
Gandhi, P
Hailey, CJ
Harrison, FA
Koss, M
Markwardt, CB
Stern, D
Treister, E
Zhang, WW
AF Ricci, C.
Bauer, F. E.
Arevalo, P.
Boggs, S.
Brandt, W. N.
Christensen, F. E.
Craig, W. W.
Gandhi, P.
Hailey, C. J.
Harrison, F. A.
Koss, M.
Markwardt, C. B.
Stern, D.
Treister, E.
Zhang, W. W.
TI IC 751: A NEW CHANGING LOOK AGN DISCOVERED BY NUSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual: (IC 751); galaxies: Seyfert;
X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; X-RAY-ABSORPTION; BROAD-BAND OBSERVATIONS;
PHOTON IMAGING CAMERA; COMPTON-THICK; XMM-NEWTON; CLUMPY-TORUS; SPECTRAL
VARIABILITY; EXTREME ABSORPTION; EMITTING REGION
AB We present results of five Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the type 2 active galactic nucleus (AGN) in IC 751, three of which were performed simultaneously with XMM-Newton or Swift/X-Ray Telescope. We find that the nuclear X-ray source underwent a clear transition from a Compton-thick (N-H similar or equal to 2 x 10(24) cm(-2)) to a Compton-thin (N-H similar or equal to 4 x 10(23) cm(-2)) state on timescales of less than or similar to 3 months, which makes IC 751 the first changing. look AGN discovered by NuSTAR. Changes of the line of sight column density at the similar to 2 sigma level are also found on a timescale of similar to 48 hr (Delta N-H similar to 10(23) cm(-2)). From the lack of spectral variability on timescales of similar to 100 ks, we infer that the varying absorber is located beyond the emission-weighted average radius of the broad-line region (BLR), and could therefore be related either to the external part of the BLR or a clumpy molecular torus. By adopting a physical torus X-ray spectral model, we are able to disentangle the column density of the non-varying absorber (N-H similar to 3.8 x 10(23) cm(-2)) from that of the varying clouds [N-H similar to (1 - 150) x 10(22) cm(-2)], and to constrain that of the material responsible for the reprocessed X-ray radiation (N-H similar to 6 x 10(24) cm(-2)). We find evidence of significant intrinsic X-ray variability, with the flux varying by a factor of five on timescales of a few months in the 2-10 and 10-50 keV band.
C1 [Ricci, C.; Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile.
[Ricci, C.; Bauer, F. E.; Treister, E.] EMBIGGEN Anillo, Concepcion, Chile.
[Bauer, F. E.] Millennium Inst Astrophys, Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Bauer, F. E.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
[Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Gran Bretana N 1111, Valparaiso, Chile.
[Boggs, S.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, 525 Davey Lab, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA.
[Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektronvej 327, DK-2800 Lyngby, Denmark.
[Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Koss, M.] ETH, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Markwardt, C. B.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Mail Code 661, Greenbelt, MD 20771 USA.
[Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Treister, E.] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile.
RP Ricci, C (reprint author), Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile.; Ricci, C (reprint author), EMBIGGEN Anillo, Concepcion, Chile.
EM cricci@astro.puc.cl
RI Boggs, Steven/E-4170-2015
OI Boggs, Steven/0000-0001-9567-4224
FU CONICYT-Chile grants "EMBIGGEN" [Anillo ACT1101]; FONDECYT [1141218,
1140304]; NuSTAR subcontract [44A-1092750]; Swiss National Science
Foundation; Ministry of Economy, Development, and Tourism's Millennium
Science Initiative [IC120009]; Ambizione fellowship [PZ00P2 154799/1];
Basal-CATA [PFB-06/2007]
FX We thank the anonymous referee for. comments. that helped us to improve
the quality of our manuscript. CR acknowledges Marko Stalevski and
Sebastien Guillot for fruitful discussions, and Chin-Shin Chang for her
comments on the manuscript. This research has made use of the NuSTAR
Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science
Data Center (ASDC, Italy) and the California Institute of Technology
(Caltech, USA). We acknowledge financial support from the CONICYT-Chile
grants "EMBIGGEN" Anillo ACT1101 (CR, ET, FEB, PA), FONDECYT 1141218
(CR, FEB), FONDECYT 1140304 (PA), Basal-CATA PFB-06/2007 (CR, ET, FEB),
NuSTAR subcontract 44A-1092750 (WNB), the Swiss National Science
Foundation and Ambizione fellowship grant PZ00P2 154799/1 (MK), and the
Ministry of Economy, Development, and Tourism's Millennium Science
Initiative through grant IC120009, awarded to The Millennium Institute
of Astrophysics, MAS (FEB). This research has made use of the NASA/IPAC
Extragalactic Database (NED) which is operated by the Jet Propulsion
Laboratory, of data obtained from the High Energy Astrophysics Science
Archive Research Center (HEASARC), provided by NASA's Goddard Space
Flight Center, and of the SIMBAD Astronomical Database which is operated
by the Centre de Donnees astronomiques de Strasbourg.
NR 82
TC 7
Z9 7
U1 2
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 5
DI 10.3847/0004-637X/820/1/5
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000005
ER
PT J
AU Rubin, A
Gal-Yam, A
De Cia, A
Horesh, A
Khazov, D
Ofek, EO
Kulkarni, SR
Arcavi, I
Manulis, I
Yaron, O
Vreeswijk, P
Kasliwal, MM
Ben-Ami, S
Perley, DA
Cao, Y
Cenko, SB
Rebbapragada, UD
Wozniak, PR
Filippenko, AV
Clubb, KI
Nugent, PE
Pan, YC
Badenes, C
Howell, DA
Valenti, S
Sand, D
Sollerman, J
Johansson, J
Leonard, DC
Horst, JC
Armen, SF
Fedrow, JM
Quimby, RM
Mazzali, P
Pian, E
Sternberg, A
Matheson, T
Sullivan, M
Maguire, K
Lazarevic, S
AF Rubin, Adam
Gal-Yam, Avishay
De Cia, Annalisa
Horesh, Assaf
Khazov, Danny
Ofek, Eran O.
Kulkarni, S. R.
Arcavi, Iair
Manulis, Ilan
Yaron, Ofer
Vreeswijk, Paul
Kasliwal, Mansi M.
Ben-Ami, Sagi
Perley, Daniel A.
Cao, Yi
Cenko, S. Bradley
Rebbapragada, Umaa D.
Wozniak, P. R.
Filippenko, Alexei V.
Clubb, K. I.
Nugent, Peter E.
Pan, Y-C.
Badenes, C.
Howell, D. Andrew
Valenti, Stefano
Sand, David
Sollerman, J.
Johansson, Joel
Leonard, Douglas C.
Horst, J. Chuck
Armen, Stephen F.
Fedrow, Joseph M.
Quimby, Robert M.
Mazzali, Paulo
Pian, Elena
Sternberg, Assaf
Matheson, Thomas
Sullivan, M.
Maguire, K.
Lazarevic, Sanja
TI TYPE II SUPERNOVA ENERGETICS AND COMPARISON OF LIGHT CURVES TO
SHOCK-COOLING MODELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernovae: general
ID P SUPERNOVAE; LUMINOUS SUPERNOVAE; CORE-COLLAPSE; PHOTOSPHERIC PHASE;
LOW-RESOLUTION; IA SUPERNOVAE; RISE-TIME; FOLLOW-UP; MASS-LOSS; BREAKOUT
AB During the first few days after explosion, Type II supernovae (SNe) are dominated by relatively simple physics. Theoretical predictions regarding early-time SN light curves in the ultraviolet (UV) and optical bands are thus quite robust. We present, for the first time, a sample of 57 R-band SN II light curves that are well-monitored during their rise, with > 5 detections during the first 10 days after discovery, and a well-constrained time of explosion to within 1-3 days. We show that the energy per unit mass (E/M) can be deduced to roughly a factor of five by comparing early-time optical data to the 2011 model of Rabinak & Waxman, while the progenitor radius cannot be determined based on R-band data alone. We find that SN II explosion energies span a range of E/M = (0.2-20) x 10(51) erg/(10 M-circle dot), and have a mean energy per unit mass of < E/M > = 0.85 x 10(51) erg/(10 M-circle dot), corrected for Malmquist bias. Assuming a small spread in progenitor masses, this indicates a large intrinsic diversity in explosion energy. Moreover, E/M is positively correlated with the amount of Ni-56 produced in the explosion, as predicted by some recent models of core-collapse SNe. We further present several empirical correlations. The peak magnitude is correlated with the decline rate (Delta m(15)), the decline rate is weakly correlated with the rise time, and the rise time is not significantly correlated with the peak magnitude. Faster declining SNe are more luminous and have longer rise times. This limits the possible power sources for such events.
C1 [Rubin, Adam; Gal-Yam, Avishay; De Cia, Annalisa; Horesh, Assaf; Khazov, Danny; Ofek, Eran O.; Manulis, Ilan; Yaron, Ofer; Vreeswijk, Paul] Weizmann Inst Sci, Dept Particle Phys & Astrophys, 234 Herzl St, Rehovot, Israel.
[Kulkarni, S. R.; Perley, Daniel A.; Cao, Yi] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Kulkarni, S. R.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA.
[Arcavi, Iair; Howell, D. Andrew; Valenti, Stefano] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
[Arcavi, Iair] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Kasliwal, Mansi M.] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA.
Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Perley, Daniel A.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
[Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA.
[Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Rebbapragada, Umaa D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Wozniak, P. R.] Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA.
[Filippenko, Alexei V.; Clubb, K. I.; Nugent, Peter E.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
[Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Pan, Y-C.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Badenes, C.] Univ Pittsburgh, Dept Phys & Astron, 3941 OHara St, Pittsburgh, PA 15260 USA.
[Badenes, C.] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, 3941 OHara St, Pittsburgh, PA 15260 USA.
[Howell, D. Andrew] Univ Calif Santa Barbara, Dept Phys, Broida Hall,Mail Code 9530, Santa Barbara, CA 93106 USA.
[Sand, David] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
[Sollerman, J.] Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden.
[Johansson, Joel] Stockholm Univ, Oskar Klein Ctr, Dept Phys, SE-10691 Stockholm, Sweden.
[Leonard, Douglas C.; Horst, J. Chuck; Armen, Stephen F.; Fedrow, Joseph M.; Quimby, Robert M.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Fedrow, Joseph M.] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan.
[Quimby, Robert M.] Univ Tokyo, UTIAS, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan.
[Mazzali, Paulo] Liverpool John Moores Univ, IC2, Astrophys Res Inst, Liverpool Sci Pk,146 Browlow Hill, Liverpool L3 5RF, Merseyside, England.
[Mazzali, Paulo; Sternberg, Assaf] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany.
[Pian, Elena] Inst Space Astrophys & Cosm Phys, INAF, Via P Gobetti 101, I-40129 Bologna, Italy.
[Pian, Elena] Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy.
[Sternberg, Assaf] Tech Univ Munich, Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany.
[Matheson, Thomas] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA.
[Sullivan, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Maguire, K.] ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Lazarevic, Sanja] Univ Belgrade, Fac Math, Dept Astron, Belgrade, Serbia.
RP Rubin, A (reprint author), Weizmann Inst Sci, Dept Particle Phys & Astrophys, 234 Herzl St, Rehovot, Israel.
EM adam.rubin@weizmann.ac.il
RI Horesh, Assaf/O-9873-2016;
OI Horesh, Assaf/0000-0002-5936-1156; Sollerman,
Jesper/0000-0003-1546-6615; Wozniak, Przemyslaw/0000-0002-9919-3310;
Sullivan, Mark/0000-0001-9053-4820
FU EU/FP7 via ERC [307260]; Quantum universe I-CORE Program by the Israeli
Committee for Planning and Budgeting; Israel Science Foundation (ISF);
Minerva grant; ISF grant; Weizmann-UK "making connections" program;
Kimmel award; ARCHES award; Willner Family Leadership Institute Ilan
Gluzman (Secaucus, NJ); Weizmann-UK; I-CORE Program of the Planning and
Budgeting Committee; EU/FP7-ERC [615929]; NSF [AST-1009571, AST-1210311,
AST-1211916]; Christopher R. Redlich Fund; TABASGO Foundation; W.M. Keck
Foundation; Robert Martin Ayers Sciences Fund; US Department of Energy,
Laboratory Directed Research and Development program; ISF; Royal
Society; US Government; Minerva; European Community
FX A.G.Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum
universe I-CORE Program by the Israeli Committee for Planning and
Budgeting and the Israel Science Foundation (ISF); by Minerva and ISF
grants; by the Weizmann-UK "making connections" program; and by Kimmel
and ARCHES awards. E.O.O. is the incumbent of the Arye Dissentshik
career development chair and is grateful for support by grants from the
Willner Family Leadership Institute Ilan Gluzman (Secaucus, NJ), ISF,
Minerva, Weizmann-UK, and the I-CORE Program of the Planning and
Budgeting Committee and the ISF. M. S. acknowledges support from the
Royal Society and EU/FP7-ERC grant No. [615929]. K. M. is grateful for a
Marie Curie Intra-European Fellowship, within the 7th European Community
Framework Programme (FP7). D.C.L., S.F.A., J.C.H., and J.M.F. are
supported by NSF grants AST-1009571 and AST-1210311, under which part of
this research (photometry data collected at MLO) was carried out. The
supernova research of A.V.F.'s group at U.C. Berkeley presented herein
is supported by Gary & Cynthia Bengier, the Christopher R. Redlich Fund,
the TABASGO Foundation, and NSF grant AST-1211916.; Research at Lick
Observatory is partially supported by a generous gift from Google. Some
of the data presented here were obtained at the W.M. Keck Observatory,
which is operated as a scientific partnership among the California
Institute of Technology, the University of California, and NASA; the
observatory was made possible by the generous financial support of the
W.M. Keck Foundation. The William Herschel Telescope is operated on the
island of La Palma by the Isaac Newton Group in the Spanish Observatorio
del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.
This research has made use of the APASS database, located at the AAVSO
web site. Funding for APASS has been provided by the Robert Martin Ayers
Sciences Fund. A portion of this work was carried out at the Jet
Propulsion Laboratory under a Research and Technology Development Grant,
under contract with the National Aeronautics and Space Administration.
US Government Support is acknowledged. LANL participation in iPTF is
supported by the US Department of Energy as part of the Laboratory
Directed Research and Development program.
NR 75
TC 8
Z9 8
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 33
DI 10.3847/0004-637X/820/1/33
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000033
ER
PT J
AU Usmanov, AV
Goldstein, ML
Matthaeus, WH
AF Usmanov, Arcadi V.
Goldstein, Melvyn L.
Matthaeus, William H.
TI A FOUR-FLUID MHD MODEL OF THE SOLAR WIND/INTERSTELLAR MEDIUM INTERACTION
WITH TURBULENCE TRANSPORT AND PICKUP PROTONS AS SEPARATE FLUID
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: magnetic fields; magnetohydrodynamics (MHD); methods: numerical;
solar wind; Sun: heliosphere; turbulence
ID INTERSTELLAR MAGNETIC-FIELD; OUTER HELIOSPHERE; TERMINATION SHOCK;
BOUNDARY-EXPLORER; WIND MODEL; 3-DIMENSIONAL FEATURES; DISTANT
HELIOSPHERE; NEUTRAL HYDROGEN; CHARGE-EXCHANGE; 2-FLUID MODEL
AB We have developed a four-fluid, three-dimensional magnetohydrodynamic model of the solar wind interaction with the local interstellar medium. The unique features of the model are: (a) a three-fluid description for the charged components of the solar wind and interstellar plasmas (thermal protons, electrons, and pickup protons), (b) the built-in turbulence transport equations based on Reynolds decomposition and coupled with the mean-flow Reynolds-averaged equations, and (c) a solar corona/solar wind model that supplies inner boundary conditions at 40 au by computing solar wind and magnetic field parameters outward from the coronal base. The three charged species are described by separate energy equations and are assumed to move with the same velocity. The fourth fluid in the model is the interstellar hydrogen which is treated by separate continuity, momentum, and energy equations and is coupled with the charged components through photoionization and charge exchange. We evaluate the effects of turbulence transport and pickup protons on the global heliospheric structure and compute the distribution of plasma, magnetic field, and turbulence parameters throughout the heliosphere for representative solar minimum and maximum conditions. We compare our results with Voyager 1 observations in the outer heliosheath and show that the relative amplitude of magnetic fluctuations just outside the heliopause is in close agreement with the value inferred from Voyager. 1 measurements by Burlaga et al. The simulated profiles of magnetic field parameters in the outer heliosheath are in qualitative agreement with the Voyager 1 observations and with the analytical model of magnetic field draping around the heliopause of Isenberg et al.
C1 [Usmanov, Arcadi V.; Matthaeus, William H.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Usmanov, Arcadi V.; Goldstein, Melvyn L.] NASA, Goddard Space Flight Ctr, Code 672,Code 673, Greenbelt, MD 20771 USA.
RP Usmanov, AV (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.; Usmanov, AV (reprint author), NASA, Goddard Space Flight Ctr, Code 672,Code 673, Greenbelt, MD 20771 USA.
EM arcadi.usmanov@nasa.gov
FU NASA LWS program [NNX13AR42G, NNX15AB88G]; NASA Heliophysics Grand
Challenges Research program [NNX14AI63G]; Solar Probe Plus ISIS project
[D99031L]; NASA High-End Computing (HEC) Program through the NASA
Advanced Supercomputing (NAS) Division at the Ames Research Center
[SMD-14-4848, SMD-15-5715]
FX We gratefully acknowledge Len Burlaga for invaluable discussions during
the course of this study. This work was supported in part by NASA LWS
program (grants NNX13AR42G and NNX15AB88G), NASA Heliophysics Grand
Challenges Research program (grant NNX14AI63G), and the Solar Probe Plus
ISIS project under subcontract D99031L. Supercomputer time allocations
were provided by the NASA High-End Computing (HEC) Program awards
SMD-14-4848 and SMD-15-5715 through the NASA Advanced Supercomputing
(NAS) Division at the Ames Research Center and the NASA Center for
Climate Simulation (NCCS) at the Goddard Space Flight Center.
NR 100
TC 3
Z9 3
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 17
DI 10.3847/0004-637X/820/1/17
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000017
ER
PT J
AU Wyper, PF
DeVore, CR
AF Wyper, P. F.
DeVore, C. R.
TI SIMULATIONS OF SOLAR JETS CONFINED BY CORONAL LOOPS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic reconnection; Sun: activity; Sun: corona
ID X-RAY JETS; EXTREME-ULTRAVIOLET JETS; H-ALPHA SURGES; MAGNETIC
RECONNECTION MODEL; FLUX EMERGENCE; ACTIVE-REGION; CHROMOSPHERIC
EVAPORATION; NUMERICAL SIMULATIONS; CURRENT SHEETS; BLOWOUT JETS
AB Coronal jets are collimated, dynamic events that occur over a broad range of spatial scales in the solar corona. In the open magnetic field of coronal holes, jets form quasi-radial spires that can extend far out into the heliosphere, while in closed-field regions the jet outflows are confined to the corona. We explore the application of the embedded-bipole model to jets occurring in closed coronal loops. In this model, magnetic free energy is injected slowly by footpoint motions that introduce twist within the closed dome of the jet source region, and is released rapidly by the onset of an ideal kink-like instability. Two length scales characterize the system: the width (N) of the jet source region and the footpoint separation (L) of the coronal loop that envelops the jet source. We find that both the conditions for initiation and the subsequent dynamics are highly sensitive to the ratio L/N. The longest-lasting and most energetic jets occur along long coronal loops with large L/N ratios, and share many of the features of open-field jets, while smaller L/N ratios produce shorter-duration, less energetic jets that are affected by reflections from the far-loop footpoint. We quantify the transition between these behaviors and show that our model replicates key qualitative and quantitative aspects of both quiet Sun and active-region loop jets. We also find that the reconnection between the closed dome and surrounding coronal loop is very extensive: the cumulative reconnected flux at least matches the total flux beneath the dome for small L/N, and is more than double that value for large L/N.
C1 [Wyper, P. F.] Oak Ridge Associated Univ, NASA, Goddard Space Flight Ctr, Heliophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[DeVore, C. R.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Wyper, PF (reprint author), Oak Ridge Associated Univ, NASA, Goddard Space Flight Ctr, Heliophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.; DeVore, CR (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM peter.f.wyper@nasa.gov; c.richard.devore@nasa.gov
RI Wyper, Peter/H-9166-2013
FU ESA; NASA
FX This work was supported by P.F.W.'s appointment to the NASA Postdoctoral
Program, administered by Oak Ridge Associated Universities through a
contract with NASA, and by C.R.D.'s participation with a NASA Living
With a Star Focused Science Team on solar jets. The computer resources
used to perform the numerical simulations were provided to C.R.D. by
NASA's High-End Computing program at the NASA Center for Climate
Simulation. Figure 1 and its animation were created using the ESA and
NASA funded Helioviewer Project. We are grateful to our colleagues Spiro
Antiochos, Judy Karpen, Etienne Pariat, and Kevin Dalmasse for numerous
helpful discussions on the topic of solar jets, to David Pontin for
ongoing discussions and insight regarding three-dimensional
reconnection, and to our anonymous referee for suggesting clarifying
changes to the original manuscript.
NR 61
TC 4
Z9 4
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2016
VL 820
IS 1
AR 77
DI 10.3847/0004-637X/820/1/77
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DH4WT
UT WOS:000372787000076
ER
PT J
AU Dasadia, S
Sun, M
Sarazin, C
Morandi, A
Markevitch, M
Wik, D
Feretti, L
Giovannini, G
Govoni, F
Vacca, V
AF Dasadia, S.
Sun, M.
Sarazin, C.
Morandi, A.
Markevitch, M.
Wik, D.
Feretti, L.
Giovannini, G.
Govoni, F.
Vacca, V.
TI A STRONG MERGER SHOCK IN ABELL 665
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual (Abell 665);
radio continuum: general; shock waves; X-rays: galaxies: clusters
ID GALAXY CLUSTERS; X-RAY; RADIO HALOS; BOW SHOCK; INTRACLUSTER MEDIUM;
MERGING CLUSTERS; BULLET CLUSTER; COLD FRONTS; CHANDRA; SAMPLE
AB Deep (103 ks) Chandra observations of Abell 665 have revealed rich structures in this merging galaxy cluster, including a strong shock and two cold fronts. The newly discovered shock has a Mach number of M = 3.0 +/- 0.6, propagating in front of a cold disrupted cloud. This makes Abell 665 the second cluster, after the Bullet cluster, where a strong merger shock of M approximate to 3 has been detected. The shock velocity from jump conditions is consistent with (2.7 +/- 0.7) x 10(3) km s(-1). The new data also reveal a prominent southern cold front with potentially heated gas ahead of it. Abell 665 also hosts a giant radio halo. There is a hint of diffuse radio emission extending to the shock at the north, which needs to be examined with better radio data. This new strong shock provides a great opportunity to study the re-acceleration model with the X-ray and radio data combined.
C1 [Dasadia, S.; Sun, M.; Morandi, A.] Univ Alabama, Dept Phys, Huntsville, AL 35816 USA.
[Sarazin, C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Markevitch, M.; Wik, D.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Wik, D.] Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA.
[Feretti, L.] INAF ORA Bologna, Via Gobetti 101, I-40129 Bologna, Italy.
[Giovannini, G.] Dipartimento Astron, Via Ranzani 1, I-40127 Bologna, Italy.
[Govoni, F.; Vacca, V.] INAF ORA Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy.
RP Dasadia, S; Sun, M (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35816 USA.
EM sbd0002@uah.edu; ms0071@uah.edu
OI Dasadia, Sarthak/0000-0001-5979-3357; Giovannini,
Gabriele/0000-0003-4916-6362
FU National Aeronautics and Space Administration (NASA) [GO2-13160A,
GO1-12169X, GO415123X, GO2-13102A]; NASA [NAS803060]
FX The support for this work was provided by the National Aeronautics and
Space Administration (NASA) through Chandra awards GO2-13160A,
GO1-12169X, GO415123X, and GO2-13102A issued by the Chandra X-ray
Observatory Center, which is operated by the Smithsonian Astrophysical
Observatory for and on behalf of NASA under contract NAS803060.
NR 42
TC 3
Z9 3
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 20
PY 2016
VL 820
IS 1
AR L20
DI 10.3847/2041-8205/820/1/L20
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8RT
UT WOS:000372352000020
ER
PT J
AU Hannah, IG
Grefenstette, BW
Smith, DM
Glesener, L
Krucker, S
Hudson, HS
Madsen, KK
Marsh, A
White, SM
Caspi, A
Shih, AY
Harrison, FA
Stern, D
Boggs, SE
Christensen, FE
Craig, WW
Hailey, CJ
Zhang, WW
AF Hannah, Iain G.
Grefenstette, Brian W.
Smith, David M.
Glesener, Lindsay
Krucker, Saem
Hudson, Hugh S.
Madsen, Kristin K.
Marsh, Andrew
White, Stephen M.
Caspi, Amir
Shih, Albert Y.
Harrison, Fiona A.
Stern, Daniel
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Hailey, Charles J.
Zhang, William W.
TI THE FIRST X-RAY IMAGING SPECTROSCOPY OF QUIESCENT SOLAR ACTIVE REGIONS
WITH NuSTAR
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: activity; Sun: corona; Sun: X-rays, gamma rays
ID HOT PLASMA; LOOPS OBSERVATIONS; ATOMIC DATABASE; CORONAL LOOPS; QUIET
SUN; EMISSION; RHESSI; HINODE; TELESCOPE; SPECTRUM
AB We present the first observations of quiescent active regions (ARs) using the Nuclear Spectroscopic Telescope Array (NuSTAR), a focusing hard X-ray telescope capable of studying faint solar emission from high-temperature and non-thermal sources. We analyze the first directly imaged and spectrally resolved X-rays above 2 keV from non-flaring ARs, observed near the west limb on 2014 November 1. The NuSTAR X-ray images match bright features seen in extreme ultraviolet and soft X-rays. The NuSTAR imaging spectroscopy is consistent with isothermal emission of temperatures 3.1-4.4 MK and emission measures 1-8 x 10(46) cm(-3). We do not observe emission above 5 MK, but our short effective exposure times restrict the spectral dynamic range. With few counts above 6 keV, we can place constraints on the presence of an additional hotter component between 5 and 12 MK of similar to 10(46) cm(-3) and similar to 10(43) cm(-3), respectively, at least an order of magnitude stricter than previous limits. With longer duration observations and a weakening solar cycle (resulting in an increased livetime), future NuSTAR observations will have sensitivity to a wider range of temperatures as well as possible non-thermal emission.
C1 [Hannah, Iain G.; Hudson, Hugh S.] Univ Glasgow, SUPA Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Grefenstette, Brian W.; Madsen, Kristin K.; Harrison, Fiona A.] CALTECH, Cahill Ctr Astrophys, 1216 E Calif Blvd, Pasadena, CA 91125 USA.
[Smith, David M.; Marsh, Andrew] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Smith, David M.; Marsh, Andrew] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Glesener, Lindsay] Univ Minnesota Twin Cities, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Glesener, Lindsay; Krucker, Saem; Hudson, Hugh S.; Boggs, Steven E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Krucker, Saem] Univ Appl Sci & Arts Northwestern Switzerland, Sch Engn, Inst Technol 4D, CH-5210 Windisch, Switzerland.
[White, Stephen M.] Air Force Res Lab, Space Vehicles Directorate, 3550 Aberdeen Ave SE, Kirtland AFB, NM 87117 USA.
[Caspi, Amir] Southwest Res Inst, Boulder, CO 80302 USA.
[Shih, Albert Y.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Hannah, IG (reprint author), Univ Glasgow, SUPA Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
EM iain.hannah@glasgow.ac.uk
RI Hannah, Iain/F-1972-2011; Boggs, Steven/E-4170-2015;
OI Hannah, Iain/0000-0003-1193-8603; Boggs, Steven/0000-0001-9567-4224;
Hudson, Hugh/0000-0001-5685-1283; Madsen, Kristin/0000-0003-1252-4891;
Caspi, Amir/0000-0001-8702-8273
FU National Aeronautics and Space Administration; NASA [NNX12AJ36G,
NNX14AG07G, NNX13AM41H, 200021-140308, NASA NNX15AK26G, NNX14AN84G]
FX This paper made use of data from the NuSTAR mission, a project led by
the California Institute of Technology, managed by the Jet Propulsion
Laboratory, funded by the National Aeronautics and Space Administration.
We thank the NuSTAR Operations, Software, and Calibration teams for
support with the execution and analysis of these observations. This
research made use of the NuSTAR Data Analysis Software (NUSTAR-DAS)
jointly developed by the ASI Science Data Center (ASDC, Italy) and the
California Institute of Technology (USA). This work is supported by:
NASA grants NNX12AJ36G, NNX14AG07G, IGH (Royal Society University
Research Fellowship), AM (NASA Earth Space Science Fellowship,
NNX13AM41H), SK (Swiss National Science Foundation, 200021-140308), AC
(NASA NNX15AK26G, NNX14AN84G). Thanks to Kim Tolbert for OSPEX help.
NR 47
TC 7
Z9 7
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 20
PY 2016
VL 820
IS 1
AR L14
DI 10.3847/2041-8205/820/1/L14
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8RT
UT WOS:000372352000014
ER
PT J
AU Hasegawa, Y
Turner, NJ
Masiero, J
Wakita, S
Matsumoto, Y
Oshino, S
AF Hasegawa, Yasuhiro
Turner, Neal J.
Masiero, Joseph
Wakita, Shigeru
Matsumoto, Yuji
Oshino, Shoichi
TI FORMING CHONDRITES IN A SOLAR NEBULA WITH MAGNETICALLY INDUCED
TURBULENCE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE magnetic fields; meteorites, meteors, meteoroids; minor planets,
asteroids: general; planets and satellites: formation; protoplanetary
disks; turbulence
ID PROTOPLANETARY DISKS; PEBBLE ACCRETION; GIANT PLANETS; DEAD ZONES; GAS
DISKS; PLANETESIMALS; GROWTH; MASS; SYSTEMS; DUST
AB Chondritic meteorites provide valuable opportunities to investigate the origins of the solar system. We explore impact jetting as a mechanism of chondrule formation and subsequent pebble accretion as a mechanism of accreting chondrules onto parent bodies of chondrites, and investigate how these two processes can account for the currently available meteoritic data. We find that when the solar nebula is <= 5 times more massive than the minimum-mass solar nebula at a similar or equal to 2-3 au and parent bodies of chondrites are <= 10(24) g (<= 500 km in radius) in the solar nebula, impact jetting and subsequent pebble accretion can reproduce a number of properties of the meteoritic data. The properties include the present asteroid belt mass, the formation timescale of chondrules, and the magnetic field strength of the nebula derived from chondrules in Semarkona. Since this scenario requires a first generation of planetesimals that trigger impact jetting and serve as parent bodies to accrete chondrules, the upper limit of parent bodies' masses leads to the following implications: primordial asteroids that were originally >= 10(24) g in mass were unlikely to contain chondrules, while less massive primordial asteroids likely had a chondrule-rich surface layer. The scenario developed from impact jetting and pebble accretion can therefore provide new insights into the origins of the solar system.
C1 [Hasegawa, Yasuhiro; Turner, Neal J.; Masiero, Joseph] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Wakita, Shigeru; Matsumoto, Yuji; Oshino, Shoichi] Natl Astron Observ Japan, Ctr Computat Astrophys, Mitaka, Tokyo 1818588, Japan.
RP Hasegawa, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM yasuhiro@caltech.edu
OI Masiero, Joseph/0000-0003-2638-720X; Matsumoto,
Yuji/0000-0002-2383-1216; Wakita, Shigeru/0000-0002-3161-3454
FU JPL/Caltech
FX The authors thank Mario Flock, Katherine Kretke, Ryuji Morishima, and
Satoshi Okuzumi for stimulating discussions, and an anonymous referee
for comments on our manuscript. This research was carried out at
JPL/Caltech, under a contract with NASA. Y.H. is supported by
JPL/Caltech.
NR 36
TC 2
Z9 2
U1 2
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 20
PY 2016
VL 820
IS 1
AR L12
DI 10.3847/2041-8205/820/1/L12
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8RT
UT WOS:000372352000012
ER
PT J
AU Jaeggli, SA
Norton, AA
AF Jaeggli, S. A.
Norton, A. A.
TI THE MAGNETIC CLASSIFICATION OF SOLAR ACTIVE REGIONS 1992-2015
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE magnetic fields; Sun: activity; sunspots
ID SUNSPOT GROUPS; DELTA-SPOTS; FLARES; DEPENDENCE
AB The purpose of this Letter is to address a blindspot in our knowledge of solar active region (AR) statistics. To the best of our knowledge, there are no published results showing the variation of the Mount Wilson magnetic classifications as a function of solar cycle based on modern observations. We show statistics for all ARs reported in the daily Solar Region Summary from 1992 January 1 to 2015 December 31. We find that the alpha and beta class ARs (including all sub-groups, e.g., beta gamma, beta delta) make up fractions of approximately 20% and 80% of the sample, respectively. This fraction is relatively constant during high levels of activity;. however, an increase in the a fraction to about 35% and and a decrease in the beta fraction to about 65% can be seen near each solar minimum and are statistically significant at the 2 sigma level. Over 30% of all ARs observed during the years of solar maxima were appended with the classifications gamma and/or delta, while these classifications account for only a fraction of a percent during the years near the solar minima. This variation in the AR types indicates that the formation of complex ARs may be due to the pileup of frequent emergence of magnetic flux during solar maximum, rather than the emergence of complex, monolithic flux structures.
C1 [Jaeggli, S. A.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA.
[Norton, A. A.] Stanford Univ, WW Hansen Expt Phys Lab, Palo Alto, CA 94305 USA.
RP Jaeggli, SA (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA.
EM sarah.jaeggli@nasa.gov
OI Jaeggli, Sarah/0000-0001-5459-2628; Norton, Aimee/0000-0003-2622-7310
NR 18
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 20
PY 2016
VL 820
IS 1
AR L11
DI 10.3847/2041-8205/820/1/L11
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8RT
UT WOS:000372352000011
ER
PT J
AU Kurczynski, P
Gawiser, E
Acquaviva, V
Bell, EF
Dekel, A
de Mello, DF
Ferguson, HC
Gardner, JP
Grogin, NA
Guo, YC
Hopkins, PF
Koekemoer, AM
Koo, DC
Lee, SK
Mobasher, B
Primack, JR
Rafelski, M
Soto, E
Teplitz, HI
AF Kurczynski, Peter
Gawiser, Eric
Acquaviva, Viviana
Bell, Eric F.
Dekel, Avishai
de Mello, Duilia F.
Ferguson, Henry C.
Gardner, Jonathan P.
Grogin, Norman A.
Guo, Yicheng
Hopkins, Philip F.
Koekemoer, Anton M.
Koo, David C.
Lee, Seong-Kook
Mobasher, Bahram
Primack, Joel R.
Rafelski, Marc
Soto, Emmaris
Teplitz, Harry I.
TI EVOLUTION OF INTRINSIC SCATTER IN THE SFR-STELLAR MASS CORRELATION AT
0.5 < z < 3
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies:
high-redshift; galaxies: statistics
ID ULTRA DEEP FIELD; STAR-FORMATION HISTORIES; EXTRAGALACTIC LEGACY SURVEY;
FORMATION RATES; FORMING GALAXIES; MAIN-SEQUENCE; PHOTOMETRIC REDSHIFTS;
LINEAR-REGRESSION; UVUDF ULTRAVIOLET; ASTRONOMICAL DATA
AB We present estimates of intrinsic scatter in the star formation rate (SFR)-stellar mass (M-*) correlation in the redshift range 0.5 < z < 3.0 and in the mass range 10(7) < M-* < 10(11)M(circle dot). We utilize photometry in the Hubble Ultradeep Field (HUDF12) and Ultraviolet Ultra Deep Field (UVUDF) campaigns and CANDELS/GOODS-S and estimate SFR, M-* from broadband spectral energy distributions and the best-available redshifts. The maximum depth of the UDF photometry (F160W 29.9 AB, 5 sigma depth) probes the SFR-M-* correlation down to M-* similar to 10(7)M(circle dot), a factor of 10-100x lower in M-* than previous studies, and comparable to dwarf galaxies in the local universe. We find the slope of the SFR-M-* relationship to be near unity at all redshifts and the normalization to decrease with cosmic time. We find a moderate increase in intrinsic scatter with cosmic time from 0.2 to 0.4 dex across the epoch of peak cosmic star formation. None of our redshift bins show a statistically significant increase in intrinsic scatter at low mass. However, it remains possible that intrinsic scatter increases at low mass on timescales shorter than similar to 100 Myr. Our results are consistent with a picture of gradual and self-similar assembly of galaxies across more than three orders of magnitude in stellar mass from as low as 10(7)M(circle dot).
C1 [Kurczynski, Peter; Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, POB 849, Piscataway, NJ 08854 USA.
[Acquaviva, Viviana] New York City Coll Technol, Brooklyn, NY 11201 USA.
[Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel.
[de Mello, Duilia F.; Gardner, Jonathan P.; Rafelski, Marc; Soto, Emmaris] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Lab Observat Cosmol, Code 665, Greenbelt, MD 20771 USA.
[de Mello, Duilia F.; Soto, Emmaris] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Ferguson, Henry C.; Grogin, Norman A.; Koekemoer, Anton M.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Guo, Yicheng; Koo, David C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Hopkins, Philip F.] CALTECH, TAPIR, Mailcode 350-17, Pasadena, CA 91125 USA.
[Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Hopkins, Philip F.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA.
[Lee, Seong-Kook] Seoul Natl Univ, Dept Phys & Astron, Ctr Explorat Origin Universe, Seoul 151742, South Korea.
[Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Primack, Joel R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Teplitz, Harry I.] CALTECH, Infrared Proc & Anal Ctr, MS 100-22, Pasadena, CA 91125 USA.
RP Kurczynski, P (reprint author), Rutgers State Univ, Dept Phys & Astron, POB 849, Piscataway, NJ 08854 USA.
OI Koekemoer, Anton/0000-0002-6610-2048; Bell, Eric/0000-0002-5564-9873
FU NASA through Space Telescope Science Institute [GO-12534]; National
Science Foundation [1055919]; NASA [NAS5-26555]
FX The authors wish to thank Aaron Clauset for discussions. Support for HST
Program GO-12534 was provided by NASA through grants from the Space
Telescope Science Institute. This material is based upon work supported
by the National Science Foundation under grant No. 1055919. This work is
based on observations taken by the CANDELS Multi-Cycle Treasury Program
with the NASA/ESA HST, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555.
NR 47
TC 7
Z9 6
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 20
PY 2016
VL 820
IS 1
AR L1
DI 10.3847/2041-8205/820/1/L1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8RT
UT WOS:000372352000001
ER
PT J
AU Yamaguchi, H
Katsuda, S
Castro, D
Williams, BJ
Lopez, LA
Slane, PO
Smith, RK
Petre, R
AF Yamaguchi, Hiroya
Katsuda, Satoru
Castro, Daniel
Williams, Brian J.
Lopez, Laura A.
Slane, Patrick O.
Smith, Randall K.
Petre, Robert
TI THE REFINED SHOCK VELOCITY OF THE X-RAY FILAMENTS IN THE RCW 86
NORTHEAST RIM
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE acceleration of particles; ISM: individual objects (RCW 86); ISM:
supernova remnants; proper motions; shock waves; X-rays: ISM
ID SUPERNOVA REMNANT RCW-86; FE-RICH EJECTA; PROPER MOTIONS;
BALMER-FILAMENTS; IA SUPERNOVA; SN 1006; EMISSION; SHELL; EFFICIENCY;
DISCOVERY
AB A precise measurement of shock velocities is crucial for constraining the mechanism and efficiency of cosmic-ray (CR) acceleration at supernova remnant (SNR) shock fronts. The northeastern rim of the SNR RCW 86 is thought to be a particularly efficient CR acceleration site, owing to the recent result in which an extremely high shock velocity of similar to 6000 km s(-1) was claimed. Here, we revisit the same SNR rim with the Chandra X-ray Observatory, 11 years after the first observation. This longer baseline than previously available allows us to determine a more accurate proper motion of the nonthermal X-ray filament, revealing a much lower velocity of 3000 +/- 340 km s(-1) (and even slower at a brighter region). Although the value has dropped to one-half of that from the previous X-ray measurement, it is still higher than the mean velocity of the H alpha filaments in this region (similar to 1200 km s(-1)). This discrepancy implies that the filaments bright in nonthermal X-rays and H alpha emission trace different velocity components, and thus a CR pressure constrained by combining the X-ray kinematics and the H alpha spectroscopy can easily be overestimated. We also measure the proper motion of the thermal X-ray filament immediately to the south of the nonthermal one. The inferred velocity (720 +/- 360 km s(-1)) is significantly lower than that of the nonthermal filament, suggesting the presence of denser ambient material, possibly a wall formed by a wind from the progenitor, which has drastically slowed down the shock.
C1 [Yamaguchi, Hiroya; Castro, Daniel; Williams, Brian J.; Petre, Robert] NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
[Yamaguchi, Hiroya] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Katsuda, Satoru] JAXA, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.
[Lopez, Laura A.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
[Lopez, Laura A.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Slane, Patrick O.; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Yamaguchi, H (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.; Yamaguchi, H (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM hiroya.yamaguchi@nasa.gov
OI Williams, Brian/0000-0003-2063-381X
FU Chandra GO Program [GO5-16072A]
FX We thank Dr. Ryo Yamazaki for helpful discussion at Harvard-Smithsonian
Center for Astrophysics. This work is supported by the Chandra GO
Program grant GO5-16072A.
NR 29
TC 2
Z9 2
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 20
PY 2016
VL 820
IS 1
AR L3
DI 10.3847/2041-8205/820/1/L3
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8RT
UT WOS:000372352000003
ER
PT J
AU Moore, JM
McKinnon, WB
Spencer, JR
Howard, AD
Schenk, PM
Beyer, RA
Nimmo, F
Singer, KN
Umurhan, OM
White, OL
Stern, SA
Ennico, K
Olkin, CB
Weaver, HA
Young, LA
Binzel, RP
Buie, MW
Buratti, BJ
Cheng, AF
Cruikshank, DP
Grundy, WM
Linscott, IR
Reitsema, HJ
Reuter, DC
Showalter, MR
Bray, VJ
Chavez, CL
Howett, CJA
Lauer, TR
Lisse, CM
Parker, AH
Porter, SB
Robbins, SJ
Runyon, K
Stryk, T
Throop, HB
Tsang, CCC
Verbiscer, AJ
Zangari, AM
Chaikin, AL
Wilhelms, DE
AF Moore, Jeffrey M.
McKinnon, William B.
Spencer, John R.
Howard, Alan D.
Schenk, Paul M.
Beyer, Ross A.
Nimmo, Francis
Singer, Kelsi N.
Umurhan, Orkan M.
White, Oliver L.
Stern, S. Alan
Ennico, Kimberly
Olkin, Cathy B.
Weaver, Harold A.
Young, Leslie A.
Binzel, Richard P.
Buie, Marc W.
Buratti, Bonnie J.
Cheng, Andrew F.
Cruikshank, Dale P.
Grundy, Will M.
Linscott, Ivan R.
Reitsema, Harold J.
Reuter, Dennis C.
Showalter, Mark R.
Bray, Veronica J.
Chavez, Carrie L.
Howett, Carly J. A.
Lauer, Tod R.
Lisse, Carey M.
Parker, Alex Harrison
Porter, S. B.
Robbins, Stuart J.
Runyon, Kirby
Stryk, Ted
Throop, Henry B.
Tsang, Constantine C. C.
Verbiscer, Anne J.
Zangari, Amanda M.
Chaikin, Andrew L.
Wilhelms, Don E.
CA New Horizons Sci Team
TI The geology of Pluto and Charon through the eyes of New Horizons
SO SCIENCE
LA English
DT Article
ID SATELLITES; NITROGEN
AB NASA's New Horizons spacecraft has revealed the complex geology of Pluto and Charon. Pluto's encounter hemisphere shows ongoing surface geological activity centered on a vast basin containing a thick layer of volatile ices that appears to be involved in convection and advection, with a crater retention age no greater than similar to 10 million years. Surrounding terrains show active glacial flow, apparent transport and rotation of large buoyant water-ice crustal blocks, and pitting, the latter likely caused by sublimation erosion and/or collapse. More enigmatic features include tall mounds with central depressions that are conceivably cryovolcanic and ridges with complex bladed textures. Pluto also has ancient cratered terrains up to similar to 4 billion years old that are extensionally faulted and extensively mantled and perhaps eroded by glacial or other processes. Charon does not appear to be currently active, but experienced major extensional tectonism and resurfacing (probably cryovolcanic) nearly 4 billion years ago. Impact crater populations on Pluto and Charon are not consistent with the steepest impactor size-frequency distributions proposed for the Kuiper belt.
C1 [Moore, Jeffrey M.; Beyer, Ross A.; Umurhan, Orkan M.; White, Oliver L.; Ennico, Kimberly; Cruikshank, Dale P.; Chavez, Carrie L.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[McKinnon, William B.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Spencer, John R.; Singer, Kelsi N.; Stern, S. Alan; Olkin, Cathy B.; Young, Leslie A.; Buie, Marc W.; Reitsema, Harold J.; Howett, Carly J. A.; Parker, Alex Harrison; Porter, S. B.; Robbins, Stuart J.; Tsang, Constantine C. C.; Zangari, Amanda M.] SW Res Inst, Boulder, CO 80302 USA.
[Howard, Alan D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA.
[Schenk, Paul M.] Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA.
[Beyer, Ross A.; Showalter, Mark R.; Chavez, Carrie L.] SETI Inst, Mountain View, CA 94043 USA.
[Nimmo, Francis] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Weaver, Harold A.; Cheng, Andrew F.; Lisse, Carey M.; Runyon, Kirby] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
[Binzel, Richard P.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Buratti, Bonnie J.] NASA, Jet Prop Lab, Pasadena, CA 91019 USA.
[Grundy, Will M.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Linscott, Ivan R.] Stanford Univ, Stanford, CA 94305 USA.
[Reuter, Dennis C.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
[Bray, Veronica J.] Univ Arizona, Tucson, AZ 85721 USA.
[Lauer, Tod R.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Stryk, Ted] Roane State Community Coll, Oak Ridge, TN 37830 USA.
[Throop, Henry B.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Verbiscer, Anne J.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Wilhelms, Don E.] US Geol Survey, 345 Middlefield Rd, Menlo Pk, CA 94025 USA.
RP Moore, JM (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
EM jeff.moore@nasa.gov
RI Hill, Matthew/H-4312-2016; Lisse, Carey/B-7772-2016; Kollmann,
Peter/C-2583-2016;
OI Hill, Matthew/0000-0002-5674-4936; Lisse, Carey/0000-0002-9548-1526;
Kollmann, Peter/0000-0002-4274-9760; Beyer, Ross/0000-0003-4503-3335
FU NASA's New Horizons project
FX We thank the many engineers who have contributed to the success of the
New Horizons mission and NASA's Deep Space Network for a decade of
excellent support to New Horizons. We thank the reviewers for close and
meticulous reading, and P. Engebretson for contribution to figure
production. S.A.S. is also affiliated with Florida Space Institute,
Uwingu LLC, Golden Spike Co., and World View Enterprises. H.J.R. is also
affiliated with B612 Foundation and Cornell Technical Service.
Supporting imagery is available in the supplementary materials. As
contractually agreed to with NASA, fully calibrated New Horizons Pluto
system data will be released via the NASA Planetary Data System at
https://pds.nasa.gov/ in a series of stages in 2016 and 2017 as the data
set is fully downlinked and calibrated. This work was supported by
NASA's New Horizons project.
NR 22
TC 21
Z9 22
U1 6
U2 26
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD MAR 18
PY 2016
VL 351
IS 6279
BP 1284
EP 1293
DI 10.1126/science.aad7055
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DG9JD
UT WOS:000372397700035
PM 26989245
ER
PT J
AU Bagenal, F
Horanyi, M
McComas, DJ
McNutt, RL
Elliott, HA
Hill, ME
Brown, LE
Delamere, PA
Kollmann, P
Krimigis, SM
Kusterer, M
Lisse, CM
Mitchell, DG
Piquette, M
Poppe, AR
Strobel, DF
Szalay, JR
Valek, P
Vandegriff, J
Weidner, S
Zirnstein, EJ
Stern, SA
Ennico, K
Olkin, CB
Weaver, HA
Young, LA
AF Bagenal, F.
Horanyi, M.
McComas, D. J.
McNutt, R. L., Jr.
Elliott, H. A.
Hill, M. E.
Brown, L. E.
Delamere, P. A.
Kollmann, P.
Krimigis, S. M.
Kusterer, M.
Lisse, C. M.
Mitchell, D. G.
Piquette, M.
Poppe, A. R.
Strobel, D. F.
Szalay, J. R.
Valek, P.
Vandegriff, J.
Weidner, S.
Zirnstein, E. J.
Stern, S. A.
Ennico, K.
Olkin, C. B.
Weaver, H. A.
Young, L. A.
CA New Horizons Sci Team
TI Pluto's interaction with its space environment: Solar wind, energetic
particles, and dust
SO SCIENCE
LA English
DT Article
ID PICK-UP IONS; NEW-HORIZONS; BOW SHOCK; COMET 67P/CHURYUMOV-GERASIMENKO;
ATMOSPHERE; ESCAPE; SYSTEM; AU; MAGNETOTAIL; MISSION
AB The New Horizons spacecraft carried three instruments that measured the space environment near Pluto as it flew by on 14 July 2015. The Solar Wind Around Pluto (SWAP) instrument revealed an interaction region confined sunward of Pluto to within about 6 Pluto radii. The region's surprisingly small size is consistent with a reduced atmospheric escape rate, as well as a particularly high solar wind flux. Observations from the Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) instrument suggest that ions are accelerated and/or deflected around Pluto. In the wake of the interaction region, PEPSSI observed suprathermal particle fluxes equal to about 1/10 of the flux in the interplanetary medium and increasing with distance downstream. The Venetia Burney Student Dust Counter, which measures grains with radii larger than 1.4 micrometers, detected one candidate impact in +/- 5 days around New Horizons' closest approach, indicating an upper limit of <4.6 kilometers(-3) for the dust density in the Pluto system.
C1 [Bagenal, F.; Horanyi, M.; Piquette, M.; Szalay, J. R.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80600 USA.
[McComas, D. J.; Elliott, H. A.; Valek, P.; Weidner, S.; Zirnstein, E. J.] SW Res Inst, 6220 Culebra Rd, San Antonio, TX 78228 USA.
[McComas, D. J.] Univ Texas San Antonio, San Antonio, TX 78249 USA.
[McNutt, R. L., Jr.; Hill, M. E.; Brown, L. E.; Kollmann, P.; Krimigis, S. M.; Kusterer, M.; Lisse, C. M.; Mitchell, D. G.; Vandegriff, J.; Weaver, H. A.] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
[Delamere, P. A.] Univ Alaska, Fairbanks, AK 99775 USA.
[Krimigis, S. M.] Acad Athens, 28 Panapistimiou, Athens 10679, Greece.
[Poppe, A. R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Strobel, D. F.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Szalay, J. R.; Stern, S. A.; Olkin, C. B.; Young, L. A.] SW Res Inst, Boulder, CO 80302 USA.
[Ennico, K.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bagenal, F (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80600 USA.
EM bagenal@colorado.edu
RI Hill, Matthew/H-4312-2016; Lisse, Carey/B-7772-2016; Kollmann,
Peter/C-2583-2016;
OI Hill, Matthew/0000-0002-5674-4936; Lisse, Carey/0000-0002-9548-1526;
Kollmann, Peter/0000-0002-4274-9760; Valek, Philip/0000-0002-2318-8750
FU NASA's New Frontiers Program; NASA's Planetary Atmospheres Program
[NNX13AG55G]
FX We thank the many contributors to the development of the SDC, SWAP, and
PEPSSI instruments and acknowledge many useful discussions with
colleagues. The New Horizons mission is supported by NASA's New
Frontiers Program. S.A.S. is also affiliated with Florida Space
Institute, Uwingu, Golden Spike, and World View Enterprises. A.R.P.
acknowledges support from NASA's Planetary Atmospheres Program (grant
NNX13AG55G). As contractually agreed to with NASA, fully calibrated New
Horizons Pluto system data will be released via the NASA Planetary Data
System (https://pds.nasa.gov/) in a series of stages in 2016 and 2017 as
the data set is fully downlinked and calibrated.
NR 54
TC 9
Z9 9
U1 5
U2 13
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD MAR 18
PY 2016
VL 351
IS 6279
AR aad9045
DI 10.1126/science.aad9045
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DG9JD
UT WOS:000372397700033
ER
PT J
AU Gladstone, GR
Stern, SA
Ennico, K
Olkin, CB
Weaver, HA
Young, LA
Summers, ME
Strobel, DF
Hinson, DP
Kammer, JA
Parker, AH
Steffl, AJ
Linscott, IR
Parker, JW
Cheng, AF
Slater, DC
Versteeg, MH
Greathouse, TK
Retherford, KD
Throop, H
Cunningham, NJ
Woods, WW
Singer, KN
Tsang, CCC
Schindhelm, E
Lisse, CM
Wong, ML
Yung, YL
Zhu, X
Curdt, W
Lavvas, P
Young, EF
Tyler, GL
AF Gladstone, G. Randall
Stern, S. Alan
Ennico, Kimberly
Olkin, Catherine B.
Weaver, Harold A.
Young, Leslie A.
Summers, Michael E.
Strobel, Darrell F.
Hinson, David P.
Kammer, Joshua A.
Parker, Alex H.
Steffl, Andrew J.
Linscott, Ivan R.
Parker, Joel Wm.
Cheng, Andrew F.
Slater, David C.
Versteeg, Maarten H.
Greathouse, Thomas K.
Retherford, Kurt D.
Throop, Henry
Cunningham, Nathaniel J.
Woods, William W.
Singer, Kelsi N.
Tsang, Constantine C. C.
Schindhelm, Eric
Lisse, Carey M.
Wong, Michael L.
Yung, Yuk L.
Zhu, Xun
Curdt, Werner
Lavvas, Panayotis
Young, Eliot F.
Tyler, G. Leonard
CA New Horizons Sci Team
TI The atmosphere of Pluto as observed by New Horizons
SO SCIENCE
LA English
DT Article
ID RADIO OCCULTATION MEASUREMENTS; STELLAR OCCULTATIONS; THERMAL STRUCTURE;
BELT MISSION; IONOSPHERE; METHANE; MODELS; SYSTEM; IMAGER; TITAN
AB Observations made during the New Horizons flyby provide a detailed snapshot of the current state of Pluto's atmosphere. Whereas the lower atmosphere (at altitudes of less than 200 kilometers) is consistent with ground-based stellar occultations, the upper atmosphere is much colder and more compact than indicated by pre-encounter models. Molecular nitrogen (N-2) dominates the atmosphere (at altitudes of less than 1800 kilometers or so), whereas methane (CH4), acetylene (C2H2), ethylene (C2H4), and ethane (C2H6) are abundant minor species and likely feed the production of an extensive haze that encompasses Pluto. The cold upper atmosphere shuts off the anticipated enhanced-Jeans, hydrodynamic-like escape of Pluto's atmosphere to space. It is unclear whether the current state of Pluto's atmosphere is representative of its average state-over seasonal or geologic time scales.
C1 [Gladstone, G. Randall; Slater, David C.; Versteeg, Maarten H.; Greathouse, Thomas K.; Retherford, Kurt D.] SW Res Inst, San Antonio, TX 78238 USA.
[Gladstone, G. Randall; Retherford, Kurt D.] Univ Texas San Antonio, San Antonio, TX 78249 USA.
[Stern, S. Alan; Olkin, Catherine B.; Young, Leslie A.; Kammer, Joshua A.; Parker, Alex H.; Steffl, Andrew J.; Parker, Joel Wm.; Singer, Kelsi N.; Tsang, Constantine C. C.; Schindhelm, Eric; Young, Eliot F.] SW Res Inst, Boulder, CO 80302 USA.
[Ennico, Kimberly] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Weaver, Harold A.; Cheng, Andrew F.; Lisse, Carey M.; Zhu, Xun] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
[Summers, Michael E.] George Mason Univ, Fairfax, VA 22030 USA.
[Strobel, Darrell F.; Throop, Henry] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Hinson, David P.] Search Extraterr Intelligence Inst, Mountain View, CA 94043 USA.
[Linscott, Ivan R.; Woods, William W.; Tyler, G. Leonard] Stanford Univ, Stanford, CA 94305 USA.
[Cunningham, Nathaniel J.] Nebraska Wesleyan Univ, Lincoln, NE 68504 USA.
[Wong, Michael L.; Yung, Yuk L.] CALTECH, Pasadena, CA 91125 USA.
[Curdt, Werner] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Lavvas, Panayotis] Univ Reims, Grp Spect Mol & Atmospher, F-51687 Reims, France.
RP Gladstone, GR (reprint author), SW Res Inst, San Antonio, TX 78238 USA.; Gladstone, GR (reprint author), Univ Texas San Antonio, San Antonio, TX 78249 USA.
EM rgladstone@swri.edu
RI Lisse, Carey/B-7772-2016; Zhu, Xun/C-2097-2016;
OI Lisse, Carey/0000-0002-9548-1526; Zhu, Xun/0000-0001-7860-6430;
Kollmann, Peter/0000-0002-4274-9760
FU Southwest Research Institute
FX We thank the NASA's New Horizons project for their excellent and
long-term support. We thank our colleagues B. Bezard, J. Erwin, F.
Forget, M. Gurwell, S. Gusewich, C. Hansen, A. Heays, K. L. Jessup, V.
Krasnopolsky, E. Lellouch, B. Lewis, B. Sicardy, G. Stark, K. Stothoff,
A. Toigo, R. Vervack, and R. Yelle for excellent advice, data, and
useful comments. We thank the reviewers for their very useful comments.
S.A.S. is also affiliated with Florida Space Institute, Uwingu, Golden
Spike Co., and World View Enterprises. N.J.C. was a paid consultant to
Southwest Research Institute. As contractually agreed to with NASA,
fully calibrated New Horizons Pluto system data will be released via the
NASA Planetary Data System at https://pds.nasa.gov in a series of stages
in 2016 and 2017 owing to the time required to fully downlink and
calibrate the data set.
NR 55
TC 18
Z9 18
U1 10
U2 32
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD MAR 18
PY 2016
VL 351
IS 6279
AR aad8866
DI 10.1126/science.aad8866
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DG9JD
UT WOS:000372397700031
ER
PT J
AU Grundy, WM
Binzel, RP
Buratti, BJ
Cook, JC
Cruikshank, DP
Ore, CMD
Earle, AM
Ennico, K
Howett, CJA
Lunsford, AW
Olkin, CB
Parker, AH
Philippe, S
Protopapa, S
Quirico, E
Reuter, DC
Schmitt, B
Singer, KN
Verbiscer, AJ
Beyer, RA
Buie, MW
Cheng, AF
Jennings, DE
Linscott, IR
Parker, JW
Schenk, PM
Spencer, JR
Stansberry, JA
Stern, SA
Throop, HB
Tsang, CCC
Weaver, HA
Weigle, GE
Young, LA
AF Grundy, W. M.
Binzel, R. P.
Buratti, B. J.
Cook, J. C.
Cruikshank, D. P.
Ore, C. M. Dalle
Earle, A. M.
Ennico, K.
Howett, C. J. A.
Lunsford, A. W.
Olkin, C. B.
Parker, A. H.
Philippe, S.
Protopapa, S.
Quirico, E.
Reuter, D. C.
Schmitt, B.
Singer, K. N.
Verbiscer, A. J.
Beyer, R. A.
Buie, M. W.
Cheng, A. F.
Jennings, D. E.
Linscott, I. R.
Parker, J. Wm.
Schenk, P. M.
Spencer, J. R.
Stansberry, J. A.
Stern, S. A.
Throop, H. B.
Tsang, C. C. C.
Weaver, H. A.
Weigle, G. E., II
Young, L. A.
CA New Horizons Sci Team
TI Surface compositions across Pluto and Charon
SO SCIENCE
LA English
DT Article
ID NEAR-INFRARED SPECTROSCOPY; CO-CONTAINING ICES; KUIPER-BELT; SATELLITE
CHARON; SOLID NITROGEN; METHANE; TRITON; HORIZONS; SYSTEM; IRRADIATION
AB The New Horizons spacecraft mapped colors and infrared spectra across the encounter hemispheres of Pluto and Charon. The volatile methane, carbon monoxide, and nitrogen ices that dominate Pluto's surface have complicated spatial distributions resulting from sublimation, condensation, and glacial flow acting over seasonal and geological time scales. Pluto's water ice "bedrock" was also mapped, with isolated outcrops occurring in a variety of settings. Pluto's surface exhibits complex regional color diversity associated with its distinct provinces. Charon's color pattern is simpler, dominated by neutral low latitudes and a reddish northern polar region. Charon's near-infrared spectra reveal highly localized areas with strong ammonia absorption tied to small craters with relatively fresh-appearing impact ejecta.
C1 [Grundy, W. M.] Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA.
[Binzel, R. P.; Earle, A. M.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Buratti, B. J.] NASA, Jet Prop Lab, La Canada Flintridge, CA 91011 USA.
[Cook, J. C.; Howett, C. J. A.; Olkin, C. B.; Parker, A. H.; Singer, K. N.; Buie, M. W.; Parker, J. Wm.; Spencer, J. R.; Stern, S. A.; Tsang, C. C. C.; Young, L. A.] SW Res Inst, Boulder, CO 80302 USA.
[Cruikshank, D. P.; Ore, C. M. Dalle; Ennico, K.; Beyer, R. A.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Ore, C. M. Dalle; Beyer, R. A.] SETT Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Lunsford, A. W.; Reuter, D. C.; Jennings, D. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Philippe, S.; Quirico, E.; Schmitt, B.] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France.
[Protopapa, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Verbiscer, A. J.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Cheng, A. F.; Weaver, H. A.] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
[Linscott, I. R.] Stanford Univ, Stanford, CA 94305 USA.
[Schenk, P. M.] Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA.
[Stansberry, J. A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Throop, H. B.] Planetary Sci Inst, Bombay, Maharashtra, India.
[Weigle, G. E., II] SW Res Inst, San Antonio, TX 28510 USA.
RP Grundy, WM (reprint author), Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA.
EM w.grundy@lowell.edu
RI quirico, eric/K-9650-2013
OI quirico, eric/0000-0003-2768-0694
FU NASA's New Horizons Project; Centre National d'Etudes Spatiales through
its "Systeme Solaire" program
FX This work was supported by NASA's New Horizons Project. Additional
support was provided by the Centre National d'Etudes Spatiales through
its "Systeme Solaire" program (E.Q., S. Philippe, and B.S.). S.A.S. is
also affiliated with Florida Space Institute, Uwingu LLC, Golden Spike
Co., and World View Enterprises. As contractually agreed to with NASA,
fully calibrated New Horizons Pluto system data will be released via the
NASA Planetary Data System at https://pds.nasa.gov/ in a series of
stages in 2016 and 2017 as the data set is fully downlinked and
calibrated.
NR 53
TC 21
Z9 22
U1 12
U2 30
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD MAR 18
PY 2016
VL 351
IS 6279
AR aad9189
DI 10.1126/science.aad9189
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DG9JD
UT WOS:000372397700034
ER
PT J
AU Weaver, HA
Buie, MW
Buratti, BJ
Grundy, WM
Lauer, TR
Olkin, CB
Parker, AH
Porter, SB
Showalter, MR
Spencer, JR
Stern, SA
Verbiscer, AJ
McKinnon, WB
Moore, JM
Robbins, SJ
Schenk, P
Singer, KN
Barnouin, OS
Cheng, AF
Ernst, CM
Lisse, CM
Lennings, DE
Lunsford, AW
Reuter, DC
Hamilton, DP
Kaufmann, DE
Ennico, K
Young, LA
Beyer, RA
Binzel, RP
Bray, VJ
Chaikin, AL
Cook, JC
Cruiksh, DP
Dalle Ore, CM
Earle, AM
Gladstone, GR
Howett, CJA
Linscott, IR
Nimmo, F
Parker, JW
Philippe, S
Protopapa, S
Reitsema, HJ
Schmitt, B
Stryk, T
Summers, ME
Tsang, CCC
Throop, HHB
White, OL
Zangari, AM
AF Weaver, H. A.
Buie, M. W.
Buratti, B. J.
Grundy, W. M.
Lauer, T. R.
Olkin, C. B.
Parker, A. H.
Porter, S. B.
Showalter, M. R.
Spencer, J. R.
Stern, S. A.
Verbiscer, A. J.
McKinnon, W. B.
Moore, J. M.
Robbins, S. J.
Schenk, P.
Singer, K. N.
Barnouin, O. S.
Cheng, A. F.
Ernst, C. M.
Lisse, C. M.
Lennings, D. E.
Lunsford, A. W.
Reuter, D. C.
Hamilton, D. P.
Kaufmann, D. E.
Ennico, K.
Young, L. A.
Beyer, R. A.
Binzel, R. P.
Bray, V. J.
Chaikin, A. L.
Cook, J. C.
Cruiksh, D. P.
Dalle Ore, C. M.
Earle, A. M.
Gladstone, G. R.
Howett, C. J. A.
Linscott, I. R.
Nimmo, F.
Parker, J. Wm.
Philippe, S.
Protopapa, S.
Reitsema, H. J.
Schmitt, B.
Stryk, T.
Summers, M. E.
Tsang, C. C. C.
Throop, H. H. B.
White, O. L.
Zangari, A. M.
TI The small satellites of Pluto as observed by New Horizons
SO SCIENCE
LA English
DT Article
ID KUIPER-BELT OBJECTS; GIANT IMPACT ORIGIN; VOLATILE LOSS; SMALL MOONS;
IMAGER; MASSES; SYSTEM; HYDRA; NIX
AB The New Horizons mission has provided resolved measurements of Pluto's moons Styx, Nix, Kerberos, and Hydra. All four are small, with equivalent spherical diameters of similar to 40 kilometers for Nix and Hydra and similar to 10 kilometers for Styx and Kerberos. They are also highly elongated, with maximum to minimum axis ratios of similar to 2. All four moons have high albedos (similar to 50 to 90%) suggestive of a water-ice surface composition. Crater densities on Nix and Hydra imply surface ages of at least 4 billion years. The small moons rotate much faster than synchronous, with rotational poles clustered nearly orthogonal to the common pole directions of Pluto and Charon. These results reinforce the hypothesis that the small moons formed in the aftermath of a collision that produced the Pluto-Charon binary.
C1 [Weaver, H. A.; Barnouin, O. S.; Cheng, A. F.; Ernst, C. M.; Lisse, C. M.] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
[Buie, M. W.; Olkin, C. B.; Parker, A. H.; Porter, S. B.; Spencer, J. R.; Stern, S. A.; Robbins, S. J.; Singer, K. N.; Kaufmann, D. E.; Young, L. A.; Cook, J. C.; Howett, C. J. A.; Parker, J. Wm.; Reitsema, H. J.; Tsang, C. C. C.; Zangari, A. M.] SW Res Inst, Boulder, CO 80302 USA.
[Buratti, B. J.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Grundy, W. M.] Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA.
[Lauer, T. R.] Natl Opt Astron Observ, Tucson, AZ 26732 USA.
[Showalter, M. R.; Beyer, R. A.] SETI Inst, Mountain View, CA 94043 USA.
[Verbiscer, A. J.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[McKinnon, W. B.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Moore, J. M.; Ennico, K.; Beyer, R. A.; Cruiksh, D. P.; Dalle Ore, C. M.; White, O. L.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Schenk, P.] Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA.
[Lennings, D. E.; Lunsford, A. W.; Reuter, D. C.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
[Hamilton, D. P.; Protopapa, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Binzel, R. P.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Bray, V. J.; Earle, A. M.] Univ Arizona, Tucson, AZ 85721 USA.
[Gladstone, G. R.] SW Res Inst, San Antonio, TX 78238 USA.
[Linscott, I. R.] Stanford Univ, Stanford, CA 94305 USA.
[Nimmo, F.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Philippe, S.; Schmitt, B.] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France.
[Stryk, T.] Roane State Community Coll, Oak Ridge, TN 37830 USA.
[Summers, M. E.] George Mason Univ, Fairfax, VA 22030 USA.
[Throop, H. H. B.] Planetary Sci Inst, Tucson, AZ 85719 USA.
RP Weaver, HA (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM hal.weaver@jhuapl.edu
RI Lisse, Carey/B-7772-2016; Ernst, Carolyn/I-4902-2012
OI Lisse, Carey/0000-0002-9548-1526;
FU NASA's New Horizons project; NASA's Origins research program; Centre
National d'Etudes Spatiales, France
FX We thank the many dedicated engineers who contributed to the success of
the New Horizons mission and NASA's Deep Space Network for a decade of
excellent support to New Horizons. This work was supported by NASA's New
Horizons project. As contractually agreed to with NASA, fully calibrated
New Horizons Pluto system data will be released via the NASA Planetary
Data System at https://pds.nasa.gov/ in a series of stages in 2016 and
2017 because of the time required to fully downlink and calibrate the
data set. Also supported by NASA's Origins research program (D.P.H.) and
Centre National d'Etudes Spatiales, France (S. Philippe and B.S.).
S.A.S. is affiliated with Florida Space Institute, Uwingu LLC, Golden
Spike Co., and World View Enterprises.
NR 23
TC 6
Z9 6
U1 4
U2 15
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD MAR 18
PY 2016
VL 351
IS 6279
AR aae0030
DI 10.1126/science.aae0030
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DG9JD
UT WOS:000372397700032
ER
PT J
AU Davies, N
Field, D
Gavaghan, D
Holbrook, SJ
Planes, S
Troyer, M
Bonsall, M
Claudet, J
Roderick, G
Schmitt, RJ
Zettler, LA
Berteaux, V
Bossin, HC
Cabasse, C
Collin, A
Deck, J
Dell, T
Dunne, J
Gates, R
Harfoot, M
Hench, JL
Hopuare, M
Kirch, P
Kotoulas, G
Kosenkov, A
Kusenko, A
Leichter, JJ
Lenihan, H
Magoulas, A
Martinez, N
Meyer, C
Stoll, B
Swalla, B
Tartakovsky, DM
Murphy, HT
Turyshev, S
Valdvinos, F
Williams, R
Wood, S
AF Davies, Neil
Field, Dawn
Gavaghan, David
Holbrook, Sally J.
Planes, Serge
Troyer, Matthias
Bonsall, Michael
Claudet, Joachim
Roderick, George
Schmitt, Russell J.
Zettler, Linda Amaral
Berteaux, Veronique
Bossin, Herve C.
Cabasse, Charlotte
Collin, Antoine
Deck, John
Dell, Tony
Dunne, Jennifer
Gates, Ruth
Harfoot, Mike
Hench, James L.
Hopuare, Marania
Kirch, Patrick
Kotoulas, Georgios
Kosenkov, Alex
Kusenko, Alex
Leichter, James J.
Lenihan, Hunter
Magoulas, Antonios
Martinez, Neo
Meyer, Chris
Stoll, Benoit
Swalla, Billie
Tartakovsky, Daniel M.
Murphy, Hinano Teavai
Turyshev, Slava
Valdvinos, Fernanda
Williams, Rich
Wood, Spencer
CA IDEA Consortium
TI Simulating social-ecological systems: the Island Digital Ecosystem
Avatars (IDEA) consortium
SO GIGASCIENCE
LA English
DT Editorial Material
DE Computational ecology; Biodiversity; Genomics; Biocode; Earth
observations; Social-ecological system; Ecosystem dynamics; Climate
change scenarios; Predictive modeling
ID INTERGOVERNMENTAL PLATFORM; MODEL; SCIENCE; BIODIVERSITY
AB Systems biology promises to revolutionize medicine, yet human wellbeing is also inherently linked to healthy societies and environments (sustainability). The IDEA Consortium is a systems ecology open science initiative to conduct the basic scientific research needed to build use-oriented simulations (avatars) of entire social-ecological systems. Islands are the most scientifically tractable places for these studies and we begin with one of the best known: Moorea, French Polynesia. The Moorea IDEA will be a sustainability simulator modeling links and feedbacks between climate, environment, biodiversity, and human activities across a coupled marine-terrestrial landscape. As a model system, the resulting knowledge and tools will improve our ability to predict human and natural change on Moorea and elsewhere at scales relevant to management/conservation actions.
C1 [Davies, Neil] Univ Calif Berkeley, Gump South Pacific Res Stn, BP 244, Moorea 98728, Fr Polynesia.
[Davies, Neil; Field, Dawn; Bonsall, Michael] Univ Oxford, Dept Zool, Biodivers Inst, Tinbergen Bldg,South Parks Rd, Oxford OX1 3PS, England.
[Davies, Neil; Cabasse, Charlotte] Univ Calif Berkeley, Berkeley Inst Data Sci, 190 Doe Lib, Berkeley, CA 94720 USA.
[Gavaghan, David] Univ Oxford, Dept Comp Sci, Computat Biol Grp, Wolfson Bldg, Oxford, England.
[Holbrook, Sally J.; Schmitt, Russell J.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA.
[Holbrook, Sally J.; Schmitt, Russell J.] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA.
[Planes, Serge; Claudet, Joachim; Berteaux, Veronique] CRIOBE, Lab Excellence CORAIL, USR CNRS EPHE UPVD 3278, BP 1013, Papetoai 98729, Moorea, Fr Polynesia.
[Troyer, Matthias; Kosenkov, Alex] Swiss Fed Inst Technol, Inst Theoret Phys & Platform Adv Sci Comput, CH-8093 Zurich, Switzerland.
[Roderick, George] Univ Calif Berkeley, Dept Environm Sci Policy & Management, 130 Mulford Hall 3114, Berkeley, CA 94720 USA.
[Zettler, Linda Amaral] Inst Marine Biol, Josephine Bay Paul Ctr Comparat Mol Biol & Evolut, Woods Hole, MA 02543 USA.
[Bossin, Herve C.] Inst Louis Malarde, Unit Med Entomol, BP 30, Tahiti 98713, Fr Polynesia.
[Collin, Antoine] Ecole Prat Hautes Etud, Lab Coastal Geomorphol & Environm, Dinard, France.
[Deck, John] Berkeley Nat Hist Museums, 3101 Valley Life Sci Bldg, Berkeley, CA 94720 USA.
[Dell, Tony] NGRREC, 1 Confluence Way, East Alton, IL 62024 USA.
[Dunne, Jennifer] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA.
[Gates, Ruth] Univ Hawaii Manoa, Hawaii Inst Marine Biol, Sch Ocean & Earth Sci & Technol, POB 1346, Kaneohe, HI 96744 USA.
[Harfoot, Mike] United Nations Environm Programme World Conservat, 219 Huntingdon Rd, Cambridge CB3 0DL, England.
[Hench, James L.] Duke Univ, Nicholas Sch Environm, Marine Lab, 135 Marine Lab Rd, Beaufort, NC 28516 USA.
[Hopuare, Marania; Stoll, Benoit] Univ Polynesie Francaise, Lab GePaSud, Tahiti BP6570, Faaa, Fr Polynesia.
[Kirch, Patrick] Univ Calif Berkeley, Dept Anthropol, 232 Kroeber Hall, Berkeley, CA 94720 USA.
[Kotoulas, Georgios; Magoulas, Antonios] Biotechnol & Aquaculture Hellen Ctr Marine Res Go, Inst Marine Biol, POB 2214, GR-71003 Iraklion, Crete, Greece.
[Kusenko, Alex] Univ Calif Los Angeles, Dept Phys & Astron, 475 Portola Plaza, Los Angeles, CA 90095 USA.
[Leichter, James J.] Univ Calif San Diego, Scripps Inst Oceanog, 9500 Gilman Dr, La Jolla, CA 92093 USA.
[Lenihan, Hunter] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, 3428 Bren Hall, Santa Barbara, CA 93106 USA.
[Martinez, Neo; Valdvinos, Fernanda] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA.
[Martinez, Neo] Pacific Ecoinformat & Computat Ecol Lab, Berkeley, CA 94703 USA.
[Meyer, Chris] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012,MRC 163, Washington, DC 20013 USA.
[Swalla, Billie] Univ Washington, Friday Harbor Labs, 620 Univ Rd, Friday Harbor, WA 98250 USA.
[Tartakovsky, Daniel M.] Univ Calif San Diego, Dept Mech & Aerosp Engn, 9500 Gilman Dr,Mail Code 0411, La Jolla, CA 92093 USA.
[Murphy, Hinano Teavai] Univ Calif Berkeley, Gump Stn, Atitia Ctr, BP 244, Moorea 98728, Fr Polynesia.
[Turyshev, Slava] CALTECH, NASA Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Turyshev, Slava] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Turyshev, Slava] Univ Calif Los Angeles, Dept Earth & Planetary Sci, Los Angeles, CA 90095 USA.
[Williams, Rich] Vibrant Data Inc, 943 Clay St, San Francisco, CA 94108 USA.
[Wood, Spencer] Univ Washington, Sch Environm & Forest Sci, Box 352100, Seattle, WA 98195 USA.
[IDEA Consortium] Swiss Fed Inst Technol, IDEA Consortium, Zurich, Switzerland.
RP Davies, N (reprint author), Univ Calif Berkeley, Gump South Pacific Res Stn, BP 244, Moorea 98728, Fr Polynesia.; Troyer, M (reprint author), Swiss Fed Inst Technol, Inst Theoret Phys & Platform Adv Sci Comput, CH-8093 Zurich, Switzerland.
EM ndavies@moorea.berkeley.edu; troyer@phys.ethz.ch
RI Claudet, Joachim/C-6335-2008; Martinez, Neo/A-5312-2008; Troyer,
Matthias/B-7826-2008; Davies, Neil/E-5863-2012;
OI Claudet, Joachim/0000-0001-6295-1061; Martinez, Neo/0000-0002-1130-5550;
Troyer, Matthias/0000-0002-1469-9444; Davies, Neil/0000-0001-8085-5014;
Collin, Antoine/0000-0001-9559-7572; BOSSIN, Herve/0000-0002-3655-0923;
gavaghan, david/0000-0001-8311-3200
NR 19
TC 1
Z9 1
U1 4
U2 30
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
EI 2047-217X
J9 GIGASCIENCE
JI GigaScience
PD MAR 17
PY 2016
VL 5
AR 14
DI 10.1186/s13742-016-0118-5
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DG9UA
UT WOS:000372428100001
PM 26998258
ER
PT J
AU Marsili, F
Stevens, MJ
Kozorezov, A
Verma, VB
Lambert, C
Stern, JA
Horansky, RD
Dyer, S
Duff, S
Pappas, DP
Lita, AE
Shaw, MD
Mirin, RP
Nam, SW
AF Marsili, F.
Stevens, M. J.
Kozorezov, A.
Verma, V. B.
Lambert, Colin
Stern, J. A.
Horansky, R. D.
Dyer, S.
Duff, S.
Pappas, D. P.
Lita, A. E.
Shaw, M. D.
Mirin, R. P.
Nam, S. W.
TI Hotspot relaxation dynamics in a current-carrying superconductor
SO PHYSICAL REVIEW B
LA English
DT Article
ID SINGLE-PHOTON DETECTORS; QUASI-PARTICLE; EFFICIENCY
AB We experimentally studied the dynamics of optically excited hotspots in current-carrying WSi superconducting nanowires as a function of bias current, bath temperature, and excitation wavelength. We observed that the hotspot relaxation time depends on bias current, temperature, and wavelength. We explained this effect with a model based on quasiparticle recombination, which provides insight into the quasiparticle dynamics of superconductors.
C1 [Marsili, F.; Stern, J. A.; Shaw, M. D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Stevens, M. J.; Verma, V. B.; Horansky, R. D.; Dyer, S.; Duff, S.; Pappas, D. P.; Lita, A. E.; Mirin, R. P.; Nam, S. W.] NIST, 325 Broadway, Boulder, CO 80305 USA.
[Kozorezov, A.; Lambert, Colin] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England.
RP Marsili, F (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM francesco.marsili.dr@jpl.nasa.gov
FU Engineering and Physical Sciences Research Council
FX Part of the research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. A.K. and C.L. gratefully
acknowledge financial support from the Engineering and Physical Sciences
Research Council.
NR 34
TC 2
Z9 2
U1 6
U2 11
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9950
EI 2469-9969
J9 PHYS REV B
JI Phys. Rev. B
PD MAR 17
PY 2016
VL 93
IS 9
AR 094518
DI 10.1103/PhysRevB.93.094518
PG 10
WC Physics, Condensed Matter
SC Physics
GA DG9KK
UT WOS:000372401300002
ER
PT J
AU Morton, DC
Nagol, J
Carabajal, CC
Rosette, J
Palace, M
Cook, BD
Vermote, EF
Harding, DJ
North, PRJ
AF Morton, Douglas C.
Nagol, Jyoteshwar
Carabajal, Claudia C.
Rosette, Jacqueline
Palace, Michael
Cook, Bruce D.
Vermote, Eric F.
Harding, David J.
North, Peter R. J.
TI Dry-season greening of Amazon forests Reply
SO NATURE
LA English
DT Letter
ID RAIN-FORESTS; VARIABILITY; SUNLIGHT
C1 [Morton, Douglas C.; Carabajal, Claudia C.; Rosette, Jacqueline; Cook, Bruce D.; Vermote, Eric F.; Harding, David J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nagol, Jyoteshwar; Rosette, Jacqueline] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Nagol, Jyoteshwar] Global Land Cover Facil, College Pk, MD 20740 USA.
[Carabajal, Claudia C.] Sigma Space Corp, Lanham, MD 20706 USA.
[Rosette, Jacqueline; North, Peter R. J.] Swansea Univ, Dept Geog, Singleton Pk, Swansea SA2 8PP, W Glam, Wales.
[Palace, Michael] Univ New Hampshire, Earth Syst Res Ctr, Durham, NH 03824 USA.
RP Morton, DC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM douglas.morton@nasa.gov
RI Morton, Douglas/D-5044-2012; North, Peter/A-1616-2009
OI North, Peter/0000-0001-9933-6935
NR 14
TC 0
Z9 0
U1 6
U2 20
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD MAR 17
PY 2016
VL 531
IS 7594
BP E6
EP E6
DI 10.1038/nature16458
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DG4TA
UT WOS:000372064300015
PM 26983545
ER
PT J
AU Cook, BI
Anchukaitis, KJ
Touchan, R
Meko, DM
Cook, ER
AF Cook, Benjamin I.
Anchukaitis, Kevin J.
Touchan, Ramzi
Meko, David M.
Cook, Edward R.
TI Spatiotemporal drought variability in the Mediterranean over the last
900years
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE drought; dendrochronology; Mediterranean; paleoclimate
ID NORTH-ATLANTIC OSCILLATION; TREE-RING WIDTH; CLIMATE-CHANGE;
HYDROLOGICAL CYCLE; DECADAL TRENDS; PRECIPITATION VARIABILITY;
ATMOSPHERIC CIRCULATION; ROBUST ESTIMATION; TIME-SERIES; RECONSTRUCTION
AB Recent Mediterranean droughts have highlighted concerns that climate change may be contributing to observed drying trends, but natural climate variability in the region is still poorly understood. We analyze 900years (1100-2012) of Mediterranean drought variability in the Old World Drought Atlas (OWDA), a spatiotemporal tree ring reconstruction of the June-July-August self-calibrating Palmer Drought Severity Index. In the Mediterranean, the OWDA is highly correlated with spring precipitation (April-June), the North Atlantic Oscillation (January-April), the Scandinavian Pattern (January-March), and the East Atlantic Pattern (April-June). Drought variability displays significant east-west coherence across the basin on multidecadal to centennial timescales and north-south antiphasing in the eastern Mediterranean, with a tendency for wet anomalies in the Black Sea region (e.g., Greece, Anatolia, and the Balkans) when coastal Libya, the southern Levant, and the Middle East are dry, possibly related to the North Atlantic Oscillation. Recent droughts are centered in the western Mediterranean, Greece, and the Levant. Events of similar magnitude in the western Mediterranean and Greece occur in the OWDA, but the recent 15year drought in the Levant (1998-2012) is the driest in the record. Estimating uncertainties using a resampling approach, we conclude that there is an 89% likelihood that this drought is drier than any comparable period of the last 900years and a 98% likelihood that it is drier than the last 500years. These results confirm the exceptional nature of this drought relative to natural variability in recent centuries, consistent with studies that have found evidence for anthropogenically forced drying in the region.
C1 [Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Cook, Benjamin I.] Lamont Doherty Earth Observ, Ocean & Climate Phys, Palisades, NY USA.
[Anchukaitis, Kevin J.] Univ Arizona, Sch Geog & Dev, Tucson, AZ USA.
[Anchukaitis, Kevin J.; Touchan, Ramzi; Meko, David M.] Univ Arizona, Tree Ring Res Lab, Tucson, AZ 85721 USA.
[Anchukaitis, Kevin J.; Cook, Edward R.] Lamont Doherty Earth Observ, Tree Ring Lab, Palisades, NY USA.
RP Cook, BI (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.; Cook, BI (reprint author), Lamont Doherty Earth Observ, Ocean & Climate Phys, Palisades, NY USA.
EM benjamin.i.cook@nasa.gov
RI Cook, Benjamin/H-2265-2012
FU NSF Paleo Perspectives on Climate Change (P2C2) program [AGS-1103450,
AGS-1103314, AGS-1341066]; NSF [AGS-0317288, AGS-0758486, AGS-0075956,
AGS-1501856, AGS-1502224]; NOAA grant [NA10OAR4310123]; NASA
FX Funding for Anchukaitis, Meko, and Touchan was provided by grants from
the NSF Paleo Perspectives on Climate Change (P2C2) program AGS-1103450,
AGS-1103314, and AGS-1341066, with additional support from the NSF
awards AGS-0317288 (Earth System History), AGS-0758486, and AGS-0075956.
Funding for the OWDA provided to E.R. Cook was by NOAA grant
NA10OAR4310123. E.R. Cook and Anchukaitis are also supported by NSF
AGS-1501856 and AGS-1502224. Support for B.I. Cook was provided by NASA.
The Old World Drought Atlas is archived and freely available from the
National Centers for Environmental Information (NCEI) at the National
Oceanic and Atmospheric Administration
(https://www.ncdc.noaa.gov/dataaccess/paleoclimatology-data). This is
Lamont contribution 7977.
NR 86
TC 14
Z9 14
U1 4
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 16
PY 2016
VL 121
IS 5
BP 2060
EP 2074
DI 10.1002/2015JD023929
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DI6HB
UT WOS:000373598700002
ER
PT J
AU Tapiador, FJ
Behrangi, A
Haddad, ZS
Katsanos, D
de Castro, M
AF Tapiador, Francisco J.
Behrangi, Ali
Haddad, Ziad S.
Katsanos, Dimitris
de Castro, Manuel
TI Disruptions in precipitation cycles: Attribution to anthropogenic
forcing
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE precipitation; CMIP5; cycles; disruptions; rainfall; wavelets
ID EARTH SYSTEM MODEL; LINE SIMULATION CHARACTERISTICS; CLIMATE MODEL;
CMIP5 MODELS; WAVELET ANALYSIS; GLOBAL PRECIPITATION; EXTREMES INDEXES;
BLACK CARBON; TIME-SERIES; MONSOON
AB Disruptions of the spatiotemporal distribution of surface precipitation that are induced by global warming may affect Earth's climate more significantly than changes in the total precipitation amount. Identifying such disruptions at global scales is not straightforward, as it requires disentangling a weak signal from comprehensive, gapless data in a 5-D configuration space whose dimensions are latitude, longitude, time, power, and period. Drawing on reliable, state-of-the-art climate model simulations from the fifth phase of the Coupled Model Intercomparison Project (CMIP5) experiments and using well-tested analytical methods, clear changes in the global precipitation cycles have been found for the simulated period 1862-2003. It has also been found that the disruptions may be attributable to anthropogenic forcing. The disruptions are relevant enough to envision significant changes in precipitation timing if human greenhouse gas emissions continue to accumulate in the future. It is noteworthy that the effects of anthropogenic forcings have been found not predominantly in the intra-annual cycles, i.e., in the short-term weather patterns that would be indicative of local effects, but rather in the interannual planetary long-term variability of the atmosphere. This suggests a global, distributed effect of the anthropogenic forcings on precipitation, which in turn is indicative of changes in the precipitation patterns linked with changes in the thermodynamics of the precipitation microphysics and to a lesser extent with the dynamical aspects of the precipitation processes.
C1 [Tapiador, Francisco J.] Univ Castilla La Mancha, Dept Environm Sci, Toledo, Spain.
[Tapiador, Francisco J.; de Castro, Manuel] Univ Castilla La Mancha, Inst Environm Sci, Toledo, Spain.
[Behrangi, Ali; Haddad, Ziad S.] NASA, CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Haddad, Ziad S.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Katsanos, Dimitris] Natl Observ Athens, Inst Environm Res & Sustainable Dev, Athens, Greece.
RP Tapiador, FJ (reprint author), Univ Castilla La Mancha, Dept Environm Sci, Toledo, Spain.; Tapiador, FJ (reprint author), Univ Castilla La Mancha, Inst Environm Sci, Toledo, Spain.
EM francisco.tapiador@uclm.es
OI Katsanos, Dimitrios/0000-0002-1969-7982
FU [CGL2013-48367-P]
FX F.J.T. and M.C. acknowledge project CGL2013-48367-P. All data used in
this paper are publicly available through the Earth System Grid-Center
for Enabling Technologies (ESG-CET), on the page http://pcmdi9.llnl.gov.
Thanks are due to the five anonymous referees who suggested further
analyses to enhance the paper.
NR 93
TC 0
Z9 0
U1 5
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 16
PY 2016
VL 121
IS 5
BP 2161
EP 2177
DI 10.1002/2015JD023406
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DI6HB
UT WOS:000373598700008
ER
PT J
AU Oreopoulos, L
Cho, N
Lee, D
Kato, S
AF Oreopoulos, Lazaros
Cho, Nayeong
Lee, Dongmin
Kato, Seiji
TI Radiative effects of global MODIS cloud regimes
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE clouds; cloud radiative effects; MODIS; cloud regimes; A-Train
ID WEATHER STATES; ATMOSPHERE; ISCCP; FLUX; AIRS
AB We update previously published Moderate Resolution Imaging Spectroradiometer (MODIS) global cloud regimes (CRs) using the latest MODIS cloud retrievals in the Collection 6 data set. We implement a slightly different derivation method, investigate the composition of the regimes, and then proceed to examine several aspects of CR radiative appearance with the aid of various radiative flux data sets. Our results clearly show that the CRs are radiatively distinct in terms of shortwave, longwave, and their combined (total) cloud radiative effect. We show that we can clearly distinguish regimes based on whether they radiatively cool or warm the atmosphere, and thanks to radiative heating profiles, to discern the vertical distribution of cooling and warming. Terra and Aqua comparisons provide information about the degree to which morning and afternoon occurrences of regimes affect the symmetry of CR radiative contribution. We examine how the radiative discrepancies among multiple irradiance data sets suffering from imperfect spatiotemporal matching depend on CR and whether they are therefore related to the complexity of cloud structure, its interpretation by different observational systems, and its subsequent representation in radiative transfer calculations.
C1 [Oreopoulos, Lazaros; Cho, Nayeong; Lee, Dongmin] NASA GSFC, Earth Sci Div, Greenbelt, MD USA.
[Cho, Nayeong] USRA, Columbia, MD USA.
[Lee, Dongmin] Morgan State Univ, Baltimore, MD 21239 USA.
[Kato, Seiji] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Oreopoulos, L (reprint author), NASA GSFC, Earth Sci Div, Greenbelt, MD USA.
EM Lazaros.Oreopoulos@nasa.gov
RI Oreopoulos, Lazaros/E-5868-2012
OI Oreopoulos, Lazaros/0000-0001-6061-6905
FU NASA's Modeling Analysis and Prediction; CloudSat/CALIPSO; Science of
Terra program; Aqua program
FX Funding from NASA's Modeling Analysis and Prediction, CloudSat/CALIPSO,
and the Science of Terra and Aqua programs is gratefully acknowledged.
Please contact the lead author for obtaining the MODIS cloud regime data
used in this paper. Data used for this paper come from the following
sources: MODIS data were obtained from https://ladsweb.nascom.nasa.gov,
CloudSat/CALIPSO data from http://www.cloudsat.cira.colostate.edu, CCCM
data from https://eosweb.larc.nasa.gov/project/ceres/cccm_table, CERES
data from https://eosweb.larc.nasa.gov/project/ceres/ceres_table, AIRS
data from http://disc.sci.gsfc.nasa.gov/uui/search/%22AIRS%22, and MERRA
data from http://disc.sci.gsfc.nasa.gov/mdisc/.
NR 31
TC 4
Z9 4
U1 1
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 16
PY 2016
VL 121
IS 5
BP 2299
EP 2317
DI 10.1002/2015JD024502
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DI6HB
UT WOS:000373598700016
ER
PT J
AU Hopkins, FM
Kort, EA
Bush, SE
Ehleringer, JR
Lai, CT
Blake, DR
Randerson, JT
AF Hopkins, Francesca M.
Kort, Eric A.
Bush, Susan E.
Ehleringer, James R.
Lai, Chun-Ta
Blake, Donald R.
Randerson, James T.
TI Spatial patterns and source attribution of urban methane in the Los
Angeles Basin
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE methane; ethane; emissions; fugitive; apportionment
ID UNITED-STATES; PIPELINE LEAKS; EMISSIONS; CALIFORNIA; ETHANE; GAS; AIR;
SYSTEMS
AB Urban areas are increasingly recognized as a globally important source of methane to the atmosphere; however, the location of methane sources and relative contributions of source sectors are not well known. Recent atmospheric measurements in Los Angeles, California, USA, show that more than a third of the city's methane emissions are unaccounted for in inventories and suggest that fugitive fossil emissions are the unknown source. We made on-road measurements to quantify fine-scale structure of methane and a suite of complementary trace gases across the Los Angeles Basin in June 2013. Enhanced methane levels were observed across the basin but were unevenly distributed in space. We identified 213 methane hot spots from unknown emission sources. We made direct measurements of ethane to methane (C2H6/CH4) ratios of known methane emission sources in the region, including cattle, geologic seeps, landfills, and compressed natural gas fueling stations, and used these ratios to determine the contribution of biogenic and fossil methane sources to unknown hot spots and to local urban background air. We found that 75% of hot spots were of fossil origin, 20% were biogenic, and 5% of indeterminate source. In regionally integrated air, we observed a wider range of C2H6/CH4 values than observed previously. Fossil fuel sources accounted for 58-65% of methane emissions, with the range depending on the assumed C2H6/CH4 ratio of source end-members and model structure. These surveys demonstrated the prevalence of fugitive methane emissions across the Los Angeles urban landscape and suggested that uninventoried methane sources were widely distributed and primarily of fossil origin.
C1 [Hopkins, Francesca M.; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Hopkins, Francesca M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kort, Eric A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Bush, Susan E.; Ehleringer, James R.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
[Ehleringer, James R.] Univ Utah, Global Change & Sustainabil Ctr, Salt Lake City, UT USA.
[Lai, Chun-Ta] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA.
[Blake, Donald R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA.
RP Hopkins, FM (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.; Hopkins, FM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM fhopkins@uci.edu
RI Kort, Eric/F-9942-2012
OI Kort, Eric/0000-0003-4940-7541
FU U.S. Department of Energy's Office of Science (BER) [DE-SC0005266]; W.
M. Keck Institute for Space Studies
FX Original geolocated, time-stamped trace gas measurements made by mobile
laboratory are provided as Data Set S1. This research is funded by the
U.S. Department of Energy's Office of Science (BER) under grant
DE-SC0005266. This work was supported in part by the W. M. Keck
Institute for Space Studies. We thank Valerie Carranza, Joshua Miu,
Mariela Ruacho, Kristal Verhulst, Josette Marrero, and Tianyang Zhu for
help with field work and Simone Meinardi for help in the laboratory.
NR 46
TC 4
Z9 4
U1 9
U2 23
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 16
PY 2016
VL 121
IS 5
BP 2490
EP 2507
DI 10.1002/2015JD024429
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DI6HB
UT WOS:000373598700027
ER
PT J
AU Bessho, N
Chen, LJ
Hesse, M
AF Bessho, N.
Chen, L. -J.
Hesse, M.
TI Electron distribution functions in the diffusion region of asymmetric
magnetic reconnection
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE magnetic reconnection; asymmetric reconnection; electron distribution
function; PIC simulation; stagnation point; diffusion region
ID ACCELERATION
AB We study electron distribution functions in a diffusion region of antiparallel asymmetric reconnection by means of particle-in-cell simulations and analytical theory. At the electron stagnation point, the electron distribution comprises a crescent-shaped population and a core component. The crescent-shaped distribution is due to electrons coming from the magnetosheath toward the stagnation point and accelerated mainly by electric field normal to the current sheet. Only a part of magnetosheath electrons can reach the stagnation point and form the crescent-shaped distribution that has a boundary of a parabolic curve. The penetration length of magnetosheath electrons into the magnetosphere is derived. We expect that satellite observations can detect crescent-shaped electron distributions during magnetopause reconnection.
C1 [Bessho, N.; Chen, L. -J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bessho, N.; Chen, L. -J.; Hesse, M.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.
RP Bessho, N (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.; Bessho, N (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.
EM naoki.bessho@nasa.gov
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU Theory and Modeling Program of the Magnetospheric Multiscale mission;
NSF [PHY-0903923, AGS-1202537, AGS-1543598]; NASA [NNX11AH03G]; NSF MRI
program [PHY-1229408]
FX The work was supported by the Theory and Modeling Program of the
Magnetospheric Multiscale mission and by NSF grants PHY-0903923,
AGS-1202537, and AGS-1543598 and by NASA grant NNX11AH03G. We
acknowledge the use of Trillian, a Cray XE6m-200 supercomputer at UNH
supported by the NSF MRI program under grant PHY-1229408, as well as
computer resources for visualization at the National Energy Research
Scientific Computing Center. The simulation data are available upon
request from the authors.
NR 17
TC 12
Z9 12
U1 3
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 16
PY 2016
VL 43
IS 5
BP 1828
EP 1836
DI 10.1002/2016GL067886
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DH9IN
UT WOS:000373109800005
ER
PT J
AU Borstad, C
Khazendar, A
Scheuchl, B
Morlighem, M
Larour, E
Rignot, E
AF Borstad, Chris
Khazendar, Ala
Scheuchl, Bernd
Morlighem, Mathieu
Larour, Eric
Rignot, Eric
TI A constitutive framework for predicting weakening and reduced
buttressing of ice shelves based on observations of the progressive
deterioration of the remnant Larsen B Ice Shelf
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ice shelf buttressing; damage mechanics; glaciology
ID WEST ANTARCTICA; WIDESPREAD; DAMAGE; CREEP; DEFORMATION; TEMPERATURE;
PROPAGATION; MECHANICS; GLACIERS; THWAITES
AB The increasing contribution of the Antarctic Ice Sheet to sea level rise is linked to reductions in ice shelf buttressing, driven in large part by basal melting of ice shelves. These ocean-driven buttressing losses are being compounded as ice shelves weaken and fracture. To date, model projections of ice sheet evolution have not accounted for weakening ice shelves. Here we present the first constitutive framework for ice deformation that explicitly includes mechanical weakening, based on observations of the progressive degradation of the remnant Larsen B Ice Shelf from 2000 to 2015. We implement this framework in an ice sheet model and are able to reproduce most of the observed weakening of the ice shelf. In addition to predicting ice shelf weakening and reduced buttressing, this new framework opens the door for improved understanding and predictions of iceberg calving, meltwater routing and hydrofracture, and ice shelf collapse.
C1 [Borstad, Chris] Univ Ctr Svalbard, Dept Arctic Geophys, Longyearbyen, Norway.
[Khazendar, Ala; Larour, Eric; Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Scheuchl, Bernd; Morlighem, Mathieu; Rignot, Eric] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
RP Borstad, C (reprint author), Univ Ctr Svalbard, Dept Arctic Geophys, Longyearbyen, Norway.
EM chris.borstad@unis.no
RI Rignot, Eric/A-4560-2014;
OI Rignot, Eric/0000-0002-3366-0481; Borstad,
Christopher/0000-0001-6992-1770
FU NASA's Cryospheric Sciences Program
FX This work was performed at the University Centre in Svalbard, the
University of California, Irvine, and the Jet Propulsion
Laboratory-California Institute of Technology, under a contract with
NASA. A.K., B.S., E.L., E.R., and M.M. were supported by grants from
NASA's Cryospheric Sciences Program. SAR data acquisitions were
coordinated through the Polar Space Task Group. The source code for the
model used in this study, the Ice Sheet System Model (ISSM), is freely
available via issm.jpl.nasa.gov. The input files and data necessary to
reproduce the results using ISSM are available from the authors upon
request (chris.borstad@unis.no).
NR 33
TC 2
Z9 2
U1 3
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 16
PY 2016
VL 43
IS 5
BP 2027
EP 2035
DI 10.1002/2015GL067365
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DH9IN
UT WOS:000373109800030
ER
PT J
AU Kneifel, S
Kollias, P
Battaglia, A
Leinonen, J
Maahn, M
Kalesse, H
Tridon, F
AF Kneifel, S.
Kollias, P.
Battaglia, A.
Leinonen, J.
Maahn, M.
Kalesse, H.
Tridon, F.
TI First observations of triple-frequency radar Doppler spectra in
snowfall: Interpretation and applications
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE radar Doppler spectrum; triple-frequency radar; snow particle scattering
ID DUAL-WAVELENGTH RADAR; AGGREGATE SNOWFLAKES; CLOUD RADAR; FALL SPEEDS;
SCATTERING; SIGNATURES; MICROPHYSICS; CAPABILITIES; LIMITATIONS;
VELOCITIES
AB The potential of multifrequency Doppler spectra to constrain precipitation microphysics has so far only been exploited for dual-frequency spectra in rain. In this study, we extend the dual-frequency concept to triple-frequency Doppler radar spectra obtained during a snowfall event which included rimed and unrimed snow aggregates. A large selection of spectra obtained from low-turbulence regions within the cloud reveals distinctly different signatures of the derived dual spectral ratios. Due to the third frequency, a characteristic curve can be derived which is almost independent of the underlying particle size distribution and velocity-size relation. This approach provides new opportunities for validating existing and future snow scattering models and reveals how the information content of triple-frequency radar data sets can be further exploited for snowfall studies.
C1 [Kneifel, S.; Maahn, M.] Univ Cologne, Inst Geophys & Meteorol, D-50931 Cologne, Germany.
[Kollias, P.] McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ, Canada.
[Battaglia, A.; Tridon, F.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Leinonen, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kalesse, H.] Leibniz Inst Tropospher Res, Leipzig, Germany.
RP Kneifel, S (reprint author), Univ Cologne, Inst Geophys & Meteorol, D-50931 Cologne, Germany.
EM skneifel@meteo.uni-koeln.de
RI Tridon, Frederic/M-4127-2013; Kneifel, Stefan/A-2044-2015; Maahn,
Maximilian/E-8363-2014;
OI Tridon, Frederic/0000-0002-0436-283X; Kneifel,
Stefan/0000-0003-2220-2968; Maahn, Maximilian/0000-0002-2580-9100;
Battaglia, Alessandro/0000-0001-9243-3484
FU German Academic Exchange Service (DAAD); U.S. Department of Energy
Atmospheric System Research (ASR) program; German Federal Ministry of
Education and Research (BMBF) [01LK1211C]
FX Work carried out by S.K. was supported by a Postdoctoral Fellowship from
the German Academic Exchange Service (DAAD); additional funding for S.K.
and P.K. was provided by the U.S. Department of Energy Atmospheric
System Research (ASR) program. The research of J.L. was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA. The development of the radar forward operator was
supported by the German Federal Ministry of Education and Research
(BMBF) within the High Definition Clouds and Precipitation for advancing
Climate Prediction (HD(CP)2) project (01LK1211C). We thank
Robin Hogan for providing his code to compute SSRG. We also acknowledge
valuable discussions with Chris Westbrook, Thorwald Stein, and Andrew
Barrett. All remote sensing and in situ data from the BAECC campaign
used in this study are available from the ARM data archive at
http://www.archive.arm.gov. The processed spectral data are available on
request from the corresponding author.
NR 35
TC 2
Z9 2
U1 4
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 16
PY 2016
VL 43
IS 5
BP 2225
EP 2233
DI 10.1002/2015GL067618
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DH9IN
UT WOS:000373109800054
ER
PT J
AU Goldberg, DL
Vinciguerra, TP
Anderson, DC
Hembeck, L
Canty, TP
Ehrman, SH
Martins, DK
Stauffer, RM
Thompson, AM
Salawitch, RJ
Dickerson, RR
AF Goldberg, Daniel L.
Vinciguerra, Timothy P.
Anderson, Daniel C.
Hembeck, Linda
Canty, Timothy P.
Ehrman, Sheryl H.
Martins, Douglas K.
Stauffer, Ryan M.
Thompson, Anne M.
Salawitch, Ross J.
Dickerson, Russell R.
TI CAMx ozone source attribution in the eastern United States using
guidance from observations during DISCOVER-AQ Maryland
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ozone
ID MODEL PERFORMANCE; PRECURSOR RELATIONSHIPS; DYNAMIC EVALUATION;
BACKGROUND OZONE; CHESAPEAKE BAY; PART I; EMISSIONS; METEOROLOGY;
CHEMISTRY; NOX
AB A Comprehensive Air-Quality Model with Extensions (CAMx) version 6.10 simulation was assessed through comparison with data acquired during NASA's 2011 Deriving Information on Surface Conditions from Column and Vertically Resolved Observations Relevant to Air Quality (DISCOVER-AQ) Maryland field campaign. Comparisons for the baseline simulation (Carbon Bond 2005 (CB05) chemistry, Environmental Protection Agency 2011 National Emissions Inventory) show a model overestimate of NOy by +86.2% and an underestimate of HCHO by -28.3%. We present a new model framework (Carbon Bond 6 Revision 2 chemistry (CB6r2), Model of Emissions of Gases and Aerosols from Nature (MEGAN) version 2.1 biogenic emissions, 50% reduction in mobile NOx, enhanced representation of isoprene nitrates) that better matches observations. The new model framework attributes 31.4% more surface ozone in Maryland to electric generating units (EGUs) and 34.6% less ozone to on-road mobile sources. Surface ozone becomes more NOx limited throughout the eastern United States compared to the baseline simulation. The baseline model therefore likely underestimates the effectiveness of anthropogenic NOx reductions as well as the current contribution of EGUs to surface ozone.
C1 [Goldberg, Daniel L.; Anderson, Daniel C.; Hembeck, Linda; Canty, Timothy P.; Salawitch, Ross J.; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Vinciguerra, Timothy P.; Ehrman, Sheryl H.] Univ Maryland, Dept Chem & Biomol Engn, College Pk, MD 20742 USA.
[Martins, Douglas K.; Stauffer, Ryan M.; Thompson, Anne M.] Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA.
[Stauffer, Ryan M.; Salawitch, Ross J.; Dickerson, Russell R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Thompson, Anne M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Salawitch, Ross J.; Dickerson, Russell R.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA.
RP Goldberg, DL (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
EM dgoldb@atmos.umd.edu
RI Anderson, Daniel/I-4398-2014; Dickerson, Russell/F-2857-2010; Salawitch,
Ross/B-4605-2009; Canty, Timothy/F-2631-2010; Thompson, Anne
/C-3649-2014;
OI Anderson, Daniel/0000-0002-9826-9811; Dickerson,
Russell/0000-0003-0206-3083; Salawitch, Ross/0000-0001-8597-5832; Canty,
Timothy/0000-0003-0618-056X; Thompson, Anne /0000-0002-7829-0920;
Stauffer, Ryan/0000-0002-8583-7795
FU Maryland Department of the Environment (MDE); NASA Air Quality Applied
Sciences Team (AQAST); NASA Aura; NASA Atmospheric Chemistry Modeling
and Analysis Program (ACMAP)
FX We would like to thank Andrew Weinheimer, Alan Fried, Ron Cohen, and
Armin Wisthaler for their observations of trace gases from the P3-B
aircraft during DISCOVER-AQ Maryland. All data from DISCOVER-AQ Maryland
can be downloaded freely from
http://www-air.larc.nasa.gov/cgi-bin/ArcView/discover-aq.dc-2011. We
would also like to thank Julie McDill and Susan Wierman from MARAMA for
preparation of the emissions. The Maryland Department of the Environment
(MDE) (G. Tad Aburn, Michael Woodman, and Jennifer Hains), the NASA Air
Quality Applied Sciences Team (AQAST), NASA Aura, and the NASA
Atmospheric Chemistry Modeling and Analysis Program (ACMAP) all funded
this research. CAMx source code has been provided by Ramboll Environ and
can be freely downloaded from http://www.camx.com.
NR 48
TC 3
Z9 3
U1 9
U2 28
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 16
PY 2016
VL 43
IS 5
BP 2249
EP 2258
DI 10.1002/2015GL067332
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA DH9IN
UT WOS:000373109800057
ER
PT J
AU Lavers, DA
Waliser, DE
Ralph, FM
Dettinger, MD
AF Lavers, David A.
Waliser, Duane E.
Ralph, F. Martin
Dettinger, Michael D.
TI Predictability of horizontal water vapor transport relative to
precipitation: Enhancing situational awareness for forecasting western
US extreme precipitation and flooding
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE hydrological extremes; atmospheric rivers; predictability
ID MADDEN-JULIAN OSCILLATION; ATMOSPHERIC RIVERS; CALIFORNIA; MOISTURE;
IMPACTS; SYSTEM
AB The western United States is vulnerable to socioeconomic disruption due to extreme winter precipitation and floods. Traditionally, forecasts of precipitation and river discharge provide the basis for preparations. Herein we show that earlier event awareness may be possible through use of horizontal water vapor transport (integrated vapor transport (IVT)) forecasts. Applying the potential predictability concept to the National Centers for Environmental Prediction global ensemble reforecasts, across 31 winters, IVT is found to be more predictable than precipitation. IVT ensemble forecasts with the smallest spreads (least forecast uncertainty) are associated with initiation states with anomalously high geopotential heights south of Alaska, a setup conducive for anticyclonic conditions and weak IVT into the western United States. IVT ensemble forecasts with the greatest spreads (most forecast uncertainty) have initiation states with anomalously low geopotential heights south of Alaska and correspond to atmospheric rivers. The greater IVT predictability could provide warnings of impending storminess with additional lead times for hydrometeorological applications.
C1 [Lavers, David A.; Waliser, Duane E.; Ralph, F. Martin; Dettinger, Michael D.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Western Weather & Water Extremes, La Jolla, CA 92093 USA.
[Lavers, David A.] European Ctr Medium Range Weather Forecasts, Shinfield Pk, Reading RG2 9AX, Berks, England.
[Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Dettinger, Michael D.] US Geol Survey, Carson City, NV USA.
RP Lavers, DA (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Western Weather & Water Extremes, La Jolla, CA 92093 USA.; Lavers, DA (reprint author), European Ctr Medium Range Weather Forecasts, Shinfield Pk, Reading RG2 9AX, Berks, England.
EM david.lavers@ecmwf.int
FU California Department of Water Resources
FX We are grateful for financial support from the California Department of
Water Resources. The ERA-Interim data were retrieved from the ECMWF data
server. DW's contribution was carried out on behalf of the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. We thank two anonymous reviewers for their comments
that helped clarify aspects of the paper.
NR 17
TC 3
Z9 3
U1 4
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 16
PY 2016
VL 43
IS 5
BP 2275
EP 2282
DI 10.1002/2016GL067765
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DH9IN
UT WOS:000373109800060
ER
PT J
AU Dessler, AE
Ye, H
Wang, T
Schoeberl, MR
Oman, LD
Douglass, AR
Butler, AH
Rosenlof, KH
Davis, SM
Portmann, RW
AF Dessler, A. E.
Ye, H.
Wang, T.
Schoeberl, M. R.
Oman, L. D.
Douglass, A. R.
Butler, A. H.
Rosenlof, K. H.
Davis, S. M.
Portmann, R. W.
TI Transport of ice into the stratosphere and the humidification of the
stratosphere over the 21st century
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE TTL; stratospheric water vapor; convective ice
ID TROPICAL TROPOPAUSE TEMPERATURES; WATER-VAPOR; ISOTOPIC COMPOSITION;
TROPOSPHERE; MODEL; CONVECTION; OZONE; CIRCULATION; TRENDS; LAYER
AB Climate models predict that tropical lower stratospheric humidity will increase as the climate warms. We examine this trend in two state-of-the-art chemistry-climate models. Under high greenhouse gas emissions scenarios, the stratospheric entry value of water vapor increases by similar to 1ppmv over the 21st century in both models. We show with trajectory runs driven by model meteorological fields that the warming tropical tropopause layer (TTL) explains 50-80% of this increase. The remainder is a consequence of trends in evaporation of ice convectively lofted into the TTL and lower stratosphere. Our results further show that within the models we examined, ice lofting is primarily important on long time scales; on interannual time scales, TTL temperature variations explain most of the variations in lower stratospheric humidity. Assessing the ability of models to realistically represent ice lofting processes should be a high priority in the modeling community.
C1 [Dessler, A. E.; Ye, H.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA.
[Wang, T.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
[Schoeberl, M. R.] Sci & Technol Corp, Columbia, MD USA.
[Oman, L. D.; Douglass, A. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Butler, A. H.; Rosenlof, K. H.; Davis, S. M.; Portmann, R. W.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Butler, A. H.; Davis, S. M.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
RP Dessler, AE (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA.
EM adessler@tamu.edu
RI Davis, Sean/C-9570-2011; Douglass, Anne/D-4655-2012; Butler,
Amy/K-6190-2012; Oman, Luke/C-2778-2009; Portmann, Robert/C-4903-2009;
Rosenlof, Karen/B-5652-2008; Dessler, Andrew/G-8852-2012; Wang,
Tao/C-2381-2011; Manager, CSD Publications/B-2789-2015
OI Davis, Sean/0000-0001-9276-6158; Butler, Amy/0000-0002-3632-0925; Oman,
Luke/0000-0002-5487-2598; Portmann, Robert/0000-0002-0279-6087;
Rosenlof, Karen/0000-0002-0903-8270; Dessler,
Andrew/0000-0003-3939-4820; Wang, Tao/0000-0003-3430-8508;
FU NSF [AGS-1261948]; NASA [NNX13AK25G]
FX This work was supported by NSF grant AGS-1261948 and NASA grant
NNX13AK25G both to Texas A&M University. Monthly data used in this paper
are archived at https://goo.gl/sjcpiJ.
NR 51
TC 3
Z9 3
U1 5
U2 22
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 16
PY 2016
VL 43
IS 5
BP 2323
EP 2329
DI 10.1002/2016GL067991
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DH9IN
UT WOS:000373109800066
ER
PT J
AU McKay, CP
Rask, JC
Detweiler, AM
Bebout, BM
Everroad, RC
Lee, JZ
Chanton, JP
Mayer, MH
Caraballo, AAL
Kapili, B
Al-Awar, M
Al-Farraj, A
AF McKay, Christopher P.
Rask, Jon C.
Detweiler, Angela M.
Bebout, Brad M.
Everroad, R. Craig
Lee, Jackson Z.
Chanton, Jeffrey P.
Mayer, Marisa H.
Caraballo, Adrian A. L.
Kapili, Bennett
Al-Awar, Meshgan
Al-Farraj, Asma
TI An Unusual Inverted Saline Microbial Mat Community in an Interdune
Sabkha in the Rub' al Khali (the Empty Quarter), United Arab Emirates
SO PLOS ONE
LA English
DT Article
ID 16S RIBOSOMAL-RNA; DEATH-VALLEY; SUBSTRATE LIMITATION; HALOPHILIC
BACTERIUM; EVAPORITE DEPOSITS; GENOME SEQUENCE; ABU-DHABI; METHANE;
MARS; BIOSIGNATURES
AB Salt flats (sabkha) are a recognized habitat for microbial life in desert environments and as analogs of habitats for possible life on Mars. Here we report on the physical setting and microbiology of interdune sabkhas among the large dunes in the Rub' al Khali (the Empty Quarter) in Liwa Oasis, United Arab Emirates. The salt flats, composed of gypsum and halite, are moistened by relatively fresh ground water. The result is a salinity gradient that is inverted compared to most salt flat communities with the hypersaline layer at the top and freshwater layers below. We describe and characterize a rich photosynthetically-based microbial ecosystem that is protected from the arid outside environment by a translucent salt crust. Gases collected from sediments under shallow ponds in the sabkha contain methane in concentrations as high as 3400 ppm. The salt crust could preserve biomarkers and other evidence for life in the salt after it dries out. Chloride-filled depressions have been identified on Mars and although surface flow of water is unlikely on Mars today, ground water is possible. Such a near surface system with modern groundwater flowing under ancient salt deposits could be present on Mars and could be accessed by surface rovers.
C1 [McKay, Christopher P.; Rask, Jon C.; Detweiler, Angela M.; Bebout, Brad M.; Everroad, R. Craig; Lee, Jackson Z.; Mayer, Marisa H.; Caraballo, Adrian A. L.; Kapili, Bennett] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Detweiler, Angela M.; Everroad, R. Craig; Lee, Jackson Z.] Bay Area Environm Res Inst, Petaluma, CA USA.
[Chanton, Jeffrey P.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Al-Awar, Meshgan] Dubai Police Acad, Res & Studies Ctr, Dubai, U Arab Emirates.
[Al-Farraj, Asma] United Arab Emirates Univ, Dept Geog, Al Ain, U Arab Emirates.
RP McKay, CP (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Chris.McKay@NASA.gov
FU NASA; NASA ASTEP Program; Arab Youth Venture Foundation
FX NASA funded this work.; This work was supported by the NASA ASTEP
Program. Field work in the UAE was part of a NASA Spaceward Bound
program and was supported by the Arab Youth Venture Foundation. We thank
Lisa LaBonte, Hussain Al Ansari, and Annie Ortiz of the AYV Foundation
and Michael Wing, Matt Reyes, and Lucinda Land for assistance in the
field activities. We also thank Claire Langford for running the gas
samples on the GC-IRMS. We thank the reviewers for the detailed and
comprehensive reviews that greatly improved the paper.
NR 57
TC 0
Z9 0
U1 7
U2 12
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD MAR 16
PY 2016
VL 11
IS 3
AR e0150342
DI 10.1371/journal.pone.0150342
PG 17
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DH1WF
UT WOS:000372574900036
PM 26982497
ER
PT J
AU Lehnert, H
Stone, RP
AF Lehnert, Helmut
Stone, Robert P.
TI Suggestion of Raspailia (Hymeraphiopsis) septentrionalis as replacement
name for Raspailia (Hymeraphiopsis) fruticosa Lehnert & Stone, 2015
SO ZOOTAXA
LA English
DT Editorial Material
C1 [Lehnert, Helmut] Eichenstr 14, D-86507 Oberottmarshausen, Germany.
[Lehnert, Helmut] GeoBioctr LMU Munchen, Richard Wagner Str 10, D-80333 Munich, Germany.
[Stone, Robert P.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Point Lena Loop, Juneau, AK 99801 USA.
RP Lehnert, H (reprint author), Eichenstr 14, D-86507 Oberottmarshausen, Germany.; Lehnert, H (reprint author), GeoBioctr LMU Munchen, Richard Wagner Str 10, D-80333 Munich, Germany.
EM Lehnert@spongetaxonomics.de
NR 1
TC 0
Z9 0
U1 0
U2 0
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD MAR 15
PY 2016
VL 4092
IS 1
BP 139
EP 139
PG 1
WC Zoology
SC Zoology
GA DK9NJ
UT WOS:000375257200009
PM 27394372
ER
PT J
AU Fuell, KK
Guyer, BJ
Kann, D
Molthan, AL
Elmer, N
AF Fuell, Kevin K.
Guyer, Brian J.
Kann, Deirdre
Molthan, Andrew L.
Elmer, Nicholas
TI Next Generation Satellite RGB Dust Imagery Leads to Operational Changes
at NWS Albuquerque
SO JOURNAL OF OPERATIONAL METEOROLOGY
LA English
DT Article
ID GOES-R; SYSTEM; FOG
AB The National Aeronautics and Space Administration/Short-term Prediction Research and Transition (SPoRT) Center has been providing unique, multispectral red-green-blue (RGB) composite imagery to operational forecasters since 2004. More recently, SPoRT has used the European Organization for the Exploitation of Meteorological Satellites "best practices" standards for RGB composites to transition a wide array of imagery for multiple uses. A "Dust" RGB product has been made available for evaluation at the National Weather Service (NWS) in Albuquerque, New Mexico (ABQ), since 2012. Several cases have occurred where forecasters were able to isolate dust plume locations for mesoscale and synoptic events during daytime and nighttime conditions. This type of imagery is a large change from the single channel imagery typically used by operational forecast staff and, therefore, can be a challenge to interpret. This paper focuses on the integration of such new imagery into operational use as well as the benefits assessed by NWS ABQ over several documented events. The primary benefits include improvements in short-term forecasts of ceiling conditions for the aviation community as well as improved decision support services and communication to the general public regarding blowing dust.
C1 [Fuell, Kevin K.] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA.
[Guyer, Brian J.; Kann, Deirdre] NOAA, Natl Weather Servce, Albuquerque, NM USA.
[Molthan, Andrew L.] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA.
[Elmer, Nicholas] Univ Alabama, Dept Atmosopher Sci, Huntsville, AL 35899 USA.
RP Fuell, KK (reprint author), Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA.; Fuell, KK (reprint author), 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM kevin.fuell@uah.edu
NR 23
TC 1
Z9 1
U1 1
U2 1
PU NATL WEATHER ASSOC
PI NORMAN
PA 350 DAVID L BOREN BLVD, STE 2750, NORMAN, OK USA
SN 2325-6184
J9 J OPER METEOROL
JI J. Oper. Meteorol.
PD MAR 15
PY 2016
VL 4
IS 6
BP 75
EP 91
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DH6MT
UT WOS:000372905500001
ER
PT J
AU Farley, KA
Martin, P
Archer, PD
Atreya, SK
Conrad, PG
Eigenbrode, JL
Fairen, AG
Franz, HB
Freissinet, C
Glavin, DP
Mahaffy, PR
Malespin, C
Ming, DW
Navarro-Gonzalez, R
Sutter, B
AF Farley, K. A.
Martin, P.
Archer, P. D., Jr.
Atreya, S. K.
Conrad, P. G.
Eigenbrode, J. L.
Fairen, A. G.
Franz, H. B.
Freissinet, C.
Glavin, D. P.
Mahaffy, P. R.
Malespin, C.
Ming, D. W.
Navarro-Gonzalez, R.
Sutter, B.
TI Light and variable Cl-37/Cl-35 ratios in rocks from Gale Crater, Mars:
Possible signature of perchlorate
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mars; Cl isotopes; perchlorate; evolved gas analysis
ID ROCKNEST AEOLIAN DEPOSIT; STABLE-ISOTOPE FRACTIONATION; EVOLVED
GAS-ANALYSIS; MARTIAN SOIL; NATURAL PERCHLORATE; CHLORINE; ORIGIN;
NITRATE; CHONDRITES; ATMOSPHERE
AB Cl isotope ratios measured on HCl thermally evolved from as-yet-unknown phases in sedimentary rocks and sand in Gale Crater provide unexpected insights to the Martian surficial Cl cycle. The seven samples yield delta Cl-37 values ranging from -1 +/- 25 parts per thousand to -51 +/- 5 parts per thousand. Five analyses from two samples of the Sheepbed mudstone (Yellowknife Bay study area) are analytically indistinguishable with a mean delta Cl-37 of -11 +/- 7 parts per thousand (1 sigma). In contrast, four mudstones/sandstones from the Kimberley and Pahrump study areas also yielded indistinguishable ratios, but with a mean delta Cl-37 of -43 +/- 6 parts per thousand. The Rocknest sand deposit gave a highly uncertain delta Cl-37 value of -7 +/- 44 parts per thousand.
These light and highly variable delta Cl-37 values are unique among known solar system materials. Two endmember models are offered to account for these observations, and in both, perchlorate, with its extreme ability to fractionate Cl isotopes, is critical. In the first model, SAM is detecting HCl from an oxychlorine compound (e.g., perchlorate) produced from volcanic gas emissions by atmospheric chemical reactions. Similar reactions in Earth's atmosphere may be responsible for the isotopically lightest known Cl outside of this study, in perchlorate from the Atacama Desert. Some of the Gale Crater delta Cl-37 values are more negative than those in Atacama perchlorate, but because reaction mechanisms and associated fractionation factors are unknown, it is impossible to assess whether this difference is prohibitive. If the negative delta Cl-37 signal is produced in this fashion, the isotopic variability among samples could arise either from variations in the relative size of the reactant chloride and product perchlorate reservoirs, or from variations in the fraction of perchlorate reduced back to chloride after deposition. Such reduction strongly enriches Cl-37 in the residual perchlorate.
Perchlorate reduction alone offers an alternative endmember model that can explain the observed data if SAM measured HCl derived from chloride. In this model isotopically normal perchlorate produced by an unspecified mechanism is reduced to chloride. Depending on the relative size of the reduced reservoir, the integrated product chloride can vary in isotopic composition from -70 parts per thousand in the first increment all the way to the starting composition if the perchlorate is fully reduced. Thus, variable degrees of perchlorate reduction can produce chloride with the appropriate delta Cl-37 range. Combination of the two endmember models, in which the perchlorate subject to post-deposition reduction is isotopically negative from atmospheric reactions, is also possible.
Determination of the phase hosting the Cl measured by SAM, an oxychlorine compound or chloride, is critical for selecting between these models, and for developing implications of the results for the Mars surficial Cl cycle. At present it is not possible to conclusively establish which phase is responsible (possibly both), but limited evidence favors the conclusion that the measured Cl derives mostly from an oxychlorine compound. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Farley, K. A.; Martin, P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Archer, P. D., Jr.; Ming, D. W.; Sutter, B.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA.
[Atreya, S. K.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Conrad, P. G.; Eigenbrode, J. L.; Franz, H. B.; Freissinet, C.; Glavin, D. P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Fairen, A. G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Franz, H. B.] Univ Maryland, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21201 USA.
[Mahaffy, P. R.; Malespin, C.] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA.
[Navarro-Gonzalez, R.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Ciudad Univ, Mexico City 04510, DF, Mexico.
[Sutter, B.] Jacobs Technol ESCG, Houston, TX USA.
RP Farley, KA (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM farley@gps.caltech.edu
RI Gonzalez, Rafael/D-1748-2009; Glavin, Daniel/D-6194-2012
OI Glavin, Daniel/0000-0001-7779-7765
FU National Aeronautics and Space Administration
FX This work was supported by the National Aeronautics and Space
Administration. This work benefited from several anonymous reviews.
NR 56
TC 6
Z9 6
U1 6
U2 25
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
EI 1385-013X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD MAR 15
PY 2016
VL 438
BP 14
EP 24
DI 10.1016/j.epsl.2015.12.013
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DE8UV
UT WOS:000370913100002
ER
PT J
AU Campagnolo, ML
Sun, QS
Liu, Y
Schaaf, C
Wang, ZS
Roman, MO
AF Campagnolo, Manuel L.
Sun, Qingsong
Liu, Yan
Schaaf, Crystal
Wang, Zhuosen
Roman, Miguel O.
TI Estimating the effective spatial resolution of the operational BRDF,
albedo, and nadir reflectance products from MODIS and VIIRS
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE BRDF; Albedo; NBAR; MODIS; VIIRS; MCD43; VNP43; Gridded spatial
resolution
ID IMAGING SPECTRORADIOMETER MODIS; LANDSAT SURFACE REFLECTANCE;
RADIATIVE-TRANSFER CODE; SNOW-FREE ALBEDO; BIDIRECTIONAL REFLECTANCE;
ATMOSPHERIC CORRECTION; VECTOR VERSION; SATELLITE DATA; EOS-MODIS;
IN-SITU
AB Satellite derived surface albedo and view-angle corrected surface reflectance products serve as the key inputs for an array of climate, biogeochemical, and hydrologic modeling efforts. This research effort is particularly focused on establishing the effective spatial resolution of the global MODIS and VIIRS Nadir BRDF-Adjusted Reflectance (NBAR) and Albedo products. The standard MODIS Products (MCD43) are created by fitting a kernel-driven, semi-empirical BRDF model to multi-date, multi-angular surface reflectance data to establish the surface reflectance anisotropy of a location. Emphasis on a particular date within the rolling multi-date period has resulted in a daily product reported on a 500 m Sinusoidal grid tiling system. While anecdotal and theoretical experiences have suggested that this product would be representative of a larger surface area than the 500 m grid, this research both quantifies that effect, and verifies that the spatial effective resolution is consistently less than 1 km for MODIS. Results for 500 m VIIRS NBAR product show an improvement of approximately 250 m in spatial effective resolution along the scan direction. In addition to their use in modeling, the MODIS BRDF/Albedo/NBAR products (and into the future with the analogous VIIRS products) are increasingly being relied upon to monitor vegetation phenology, identify land cover and land cover disturbance, track snow fall and melt, and establish surface energy balance variability. Thus, this research provides the quantification both for MODIS and VIIRS necessary for the effective use of these products by the global modeling and monitoring communities. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Campagnolo, Manuel L.] Univ Lisbon, Sch Agr, Forest Res Ctr, P-1349017 Lisbon, Portugal.
[Campagnolo, Manuel L.] Univ Lisbon, Sch Agr, Dept Biosyst Sci & Engn, P-1349017 Lisbon, Portugal.
[Sun, Qingsong; Liu, Yan; Schaaf, Crystal] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA.
[Wang, Zhuosen; Roman, Miguel O.] NASA Goddard Space Flight Ctr, Terr Informat Syst Lab, Code 619, Greenbelt, MD 20771 USA.
[Wang, Zhuosen] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Campagnolo, ML (reprint author), Univ Lisbon, Sch Agr, Forest Res Ctr, P-1349017 Lisbon, Portugal.; Campagnolo, ML (reprint author), Univ Lisbon, Sch Agr, Dept Biosyst Sci & Engn, P-1349017 Lisbon, Portugal.
RI Sun, Qingsong/I-9040-2016;
OI Sun, Qingsong/0000-0002-7710-2123; Campagnolo,
Manuel/0000-0002-9634-3061
FU Portuguese Fundacao para a Ciencia e a Tecnologia (FCT)
[PEst-OE/AGR/UI0239/2014, UID/AGR/00239/2013]; NASA [NNX14AI73G,
NNX14AQ18A]
FX MLC was supported by the Portuguese Fundacao para a Ciencia e a
Tecnologia (FCT) through projects PEst-OE/AGR/UI0239/2014 and
UID/AGR/00239/2013. This effort was also supported by the NASA
NNX14AI73G and NNX14AQ18A. We wish to thanks all three reviewers for
their useful comments and suggestions.
NR 60
TC 3
Z9 3
U1 5
U2 19
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAR 15
PY 2016
VL 175
BP 52
EP 64
DI 10.1016/j.rse.2015.12.033
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DF0AC
UT WOS:000371000000005
ER
PT J
AU Casas, A
Garcia, M
Siegel, RB
Koltunov, A
Ramirez, C
Ustin, S
AF Casas, Angeles
Garcia, Mariano
Siegel, Rodney B.
Koltunov, Alexander
Ramirez, Carlos
Ustin, Susan
TI Burned forest characterization at single-tree level with airborne laser
scanning for assessing wildlife habitat
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Gaussian processes; Watershed segmentation; Single-tree level; Stem
diameter; Basal area; Megafire; Wildlife habitat; Black-backed
woodpecker; Airborne laser scanning; LiDAR; Snags; Dead trees; Rim fire
ID DISCRETE-RETURN LIDAR; AVIAN SPECIES RICHNESS; COARSE WOODY DEBRIS;
WOODPECKER HABITAT; INDIVIDUAL TREES; SMALL-FOOTPRINT; BIRD; FIRE;
INTENSITY; AREA
AB Abundance, size, and spatial distribution of standing dead trees (snags), are key indicators of forest biodiversity and ecosystem health. These metrics represent critical habitat components for various wildlife species of conservation concern, including the Black-backed Woodpecker (Picoides arcticus), which is strongly associated with recently burned conifer forest. We assessed the potential of Airborne Laser Scanning (ALS) to detect and characterize conifer snags and identify Black-backed Woodpecker habitat using previously derived empirical thresholds of conifer snag basal area. Over the footprint of the Rim Fire, a megafire that extended (similar to 104,000 ha) through a heterogeneous mosaic of conifer forests, oak woodlands, and meadows in the Sierra Nevada mountains of California, we identified conifer snags and estimated their basal area from single-tree ALS-derived metrics using Gaussian processes in four major steps. First, individual trees were mapped using the Watershed Segmentation algorithm, resulting in 87% detection of trees with stem diameter larger than 30 cm. Second, the snag/live classification model identified snags with an overall accuracy of 91.8%, using the coefficient of variation of height and intensity together with maximum intensity and fractional cover as the most relevant metrics. Third, the conifer/hardwood snag classification model utilizing the maximum height, median height, minimum intensity, and area metrics separated snag forest types with an overall accuracy of 84.8%. Finally, a Gaussian process regression model reliably estimated conifer snag stem diameter (R-2 = 0.81) using height and crown area, thus significantly outperforming regionally calibrated conifer-specific allometric equations. As a result,-80% of the snag basal area have been mapped. Optimal and potential habitat for Black-backed Woodpecker comprise 53.7 km(2) and 58.4 km(2), respectively, representing 5.1 and 5.6% of the footprint of the Rim Fire. Our study illustrates the utility of high-density ALS data for characterizing recently burned forests, which, in conjunction with information about the habitat needs of particular snag-dependent wildlife species, can be used to assess habitat characteristics, and thus contribute greatly to forest management and biodiversity conservation. (c) 2016 Elsevier Inc. All rights reserved.
C1 [Casas, Angeles; Koltunov, Alexander; Ustin, Susan] Univ Calif Davis, Dept Land Air & Water Resources, One Shields Ave, Davis, CA 95616 USA.
[Garcia, Mariano] Univ Leicester, Ctr Landscape & Climate Res, Univ Rd, Leicester LE1 7RH, Leics, England.
[Garcia, Mariano] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Siegel, Rodney B.] Inst Bird Populat, Point Reyes Stn, CA USA.
[Koltunov, Alexander; Ramirez, Carlos] US Forest Serv, USDA, Reg Remote Sensing Lab 5, Mcclellan, CA USA.
RP Casas, A (reprint author), Univ Calif Davis, Dept Land Air & Water Resources, One Shields Ave, Davis, CA 95616 USA.
FU USFS; Marie Curie IOF (ForeStMap-3D Forest Structure Monitoring and
Mapping) [629376]
FX This research was carried out within the ambit of the project Multi
sensor remote sensing study of California's Rim Fire to inform post-fire
ecosystem restoration and effective prevention of future catastrophic
wildfires. Sponsor: USFS. Mariano Garcia is supported by the Marie Curie
IOF (ForeStMap-3D Forest Structure Monitoring and Mapping, Project
Reference: 629376). The contents on this paper reflect only the authors
views and not the views of the European Commission. We greatly
appreciate the help of Mitzi Thornley and the Science Division Yosemite
National Park for the permission to conduct research in Yosemite
National Park (YOSE-00653/YOSE-2014-SCI-0124).
NR 76
TC 4
Z9 4
U1 7
U2 28
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAR 15
PY 2016
VL 175
BP 231
EP 241
DI 10.1016/j.rse.2015.12.044
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DF0AC
UT WOS:000371000000020
ER
PT J
AU Mira, M
Olioso, A
Gallego-Elvira, B
Courault, D
Garrigues, S
Marloie, O
Hagolle, O
Guillevic, P
Boulet, G
AF Mira, Maria
Olioso, Albert
Gallego-Elvira, Belen
Courault, Dominique
Garrigues, Sebastien
Marloie, Olivier
Hagolle, Olivier
Guillevic, Pierre
Boulet, Gilles
TI Uncertainty assessment of surface net radiation derived from Landsat
images
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Uncertainty analysis; Net radiation; Surface temperature; Albedo;
Emissivity; Landsat; Regional scale; Temporal course
ID THERMAL-INFRARED DATA; DIFFERENCE VEGETATION INDEX; RADIOMETER SUITE
VIIRS; ENERGY BALANCE MODEL; IN-SITU MEASUREMENTS; REMOTE-SENSING DATA;
NARROW-BAND; BIDIRECTIONAL REFLECTANCE; ATMOSPHERIC CORRECTION;
TEMPERATURE RETRIEVAL
AB The net radiation flux available at the Earth's surface drives evapotranspiration, photosynthesis and other physical and biological processes. The only cost-effective way to capture its spatial and temporal variability at regional and global scales is remote sensing. However, the accuracy of net radiation derived from remote sensing data has been evaluated up to now over a limited number of in situ measurements and ecosystems. This study aims at evaluating estimates and uncertainties on net radiation derived from Landsat-7 images depending on reliability of the input surface variables albedo, emissivity and surface temperature. The later includes the reliability of remote sensing information (spectral reflectances and top of canopy brightness temperature) and shortwave and longwave incoming radiations.
Primary information describing the surface is derived from remote sensing observations. Surface albedo is estimated from spectral reflectances using a narrow-to-broadband conversion method. Land surface temperature is retrieved from top of canopy brightness temperature by accounting for land surface emissivity and reflection of atmospheric radiation; and emissivity is estimated using a relationship with a vegetation index and a spectral database of soil and plant canopy properties in the study area. The net radiation uncertainty is assessed using comparison with ground measurements over the Crau-Camargue and lower Rhone valley regions in France. We found Root Mean Square Errors between retrievals and field measurements of 0.25-033 (14-19%) for albedo, similar to 1.7 K for surface temperature and similar to 20 W.m(-2) (5%) for net radiation. Results show a substantial underestimation of Landsat-7 albedo (up to 0.024), particularly for estimates retrieved using the middle infrared, which could be due to different sources: the calibration of field sensors, the correction of radiometric signals from Landsat-7 or the differences in spectral bands with the sensors for which the models where originally derived, or the atmospheric corrections. We report a global uncertainty in net radiation of 40-100 W.m(-2) equally distributed over the shortwave and longwave radiation, which varies spatially and temporally depending on the land use and the time of year. In situ measurements of incoming shortwave and longwave radiation contribute the most to uncertainty in net radiation (10-40 W.m(-2) and 20-30 W.m(-2), respectively), followed by uncertainties in albedo (<25 W.m(-2)) and surface temperature (similar to 8 W.m(-2)). For the latter, the main factors were the uncertainties in top of canopy reflectances (<10 W.m(-2)) and brightness temperature (5-7 W.m(-2)). The generalization of these results to other sensors and study regions could be considered, except for the emissivity if prior knowledge on its characterization is not available. (c) 2016 Elsevier Inc. All rights reserved.
C1 [Mira, Maria; Olioso, Albert; Courault, Dominique; Garrigues, Sebastien] INRA, French Natl Inst Agr Res, UMR EMMAH 1114, F-84914 Avignon 9, France.
[Mira, Maria; Olioso, Albert; Courault, Dominique; Garrigues, Sebastien] UAPV, UMR EMMAH 1114, F-84000 Avignon, France.
[Mira, Maria] UAB, Dept Geog, Grumets Res Grp, Bellaterra 08193, Catalonia, Spain.
[Gallego-Elvira, Belen] NERC Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England.
[Marloie, Olivier] INRA, French Natl Inst Agr Res, UR URFM 0629, F-84914 Avignon, France.
[Hagolle, Olivier; Boulet, Gilles] CESBIO, BPI 811,18 Ave E Berlin, F-31401 Toulouse 9, France.
[Guillevic, Pierre] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Mira, M (reprint author), INRA, French Natl Inst Agr Res, UMR EMMAH 1114, F-84914 Avignon 9, France.
EM Maria.Mira@uab.cat
RI Boulet, Gilles/C-3067-2013;
OI Boulet, Gilles/0000-0002-3905-7560; Mira, Maria/0000-0002-9303-8301
FU National Centre for Space Studies; CNES (TOSCA); European SIRRIMED
(Sustainable use of irrigation water in the Mediterranean) FP7 project;
Ramon Areces Foundation
FX This work was made through different projects funded by the National
Centre for Space Studies, CNES (TOSCA) and the European SIRRIMED
(Sustainable use of irrigation water in the Mediterranean) FP7 project
(www.sirrimed.org). Mira was endorsed by a postdoctoral contract within
the VALi + d program from Generalitat Valenciana (Spain), followed by a
CNES postdoctoral contract and a "Juan de la Cierva" postdoctoral
contract from the Spanish Ministry of Economy and Competitiveness.
Gallego-Elvira was endorsed by a postdoctoral fellowship from the Ramon
Areces Foundation.
NR 104
TC 6
Z9 6
U1 5
U2 28
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAR 15
PY 2016
VL 175
BP 251
EP 270
DI 10.1016/j.rse.2015.12.054
PG 20
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DF0AC
UT WOS:000371000000022
ER
PT J
AU Daubar, IJ
Dundas, CM
Byrne, S
Geissler, P
Bart, GD
McEwen, AS
Russell, PS
Chojnacki, M
Golombek, MP
AF Daubar, I. J.
Dundas, C. M.
Byrne, S.
Geissler, P.
Bart, G. D.
McEwen, A. S.
Russell, P. S.
Chojnacki, M.
Golombek, M. P.
TI Changes in blast zone albedo patterns around new martian impact craters
SO ICARUS
LA English
DT Article
DE Impact processes; Aeolian processes; Cratering; Mars; Mars, surface
ID SCIENCE EXPERIMENT HIRISE; MARS ORBITER CAMERA; SLOPE STREAKS;
LUNAR-SURFACE; STRUCTURAL DISTURBANCES; DUST; EXPLORATION; SPACECRAFT
AB "Blast zones" (BZs) around new martian craters comprise various albedo features caused by the initial impact, including diffuse halos, extended linear and arcuate rays, secondary craters, ejecta patterns, and dust avalanches. We examined these features for changes in repeat images separated by up to four Mars years. Here we present the first comprehensive survey of the qualitative and quantitative changes observed in impact blast zones over time. Such changes are most likely due to airfall of high-albedo dust restoring darkened areas to their original albedo, the albedo of adjacent non-impacted surfaces. Although some sites show drastic changes over short timescales, nearly half of the sites show no obvious changes over several Mars years. Albedo changes are more likely to occur at higher-latitude sites, lower-elevation sites, and at sites with smaller central craters. No correlation was seen between amount of change and Dust Cover Index, relative halo size, or historical regional albedo changes. Quantitative albedo measurements of the diffuse dark halos relative to their surroundings yielded estimates of fading lifetimes for these features. The average lifetime among sites with measurable fading is similar to 15 Mars years; the median is similar to 8 Mars years for a linear brightening. However, at approximately half of sites with three or more repeat images, a nonlinear function with rapid initial fading followed by a slow increase in albedo provides a better fit to the fading behavior; this would predict even longer lifetimes. The predicted lifetimes of BZs are comparable to those of slope streaks, and considered representative of fading by global atmospheric dust deposition; they last significantly longer than dust devil or rover tracks, albedo features that are erased by different processes. These relatively long lifetimes indicate that the measurement of the current impact rate by Daubar et al. (Daubar, I.J. et al. [2013]. Icarus 225, 506-516. http://dx.doi.org/ 10.1016/j.icarus.2013.04.009) does not suffer significantly from overall under-sampling due to blast zones fading before new impact sites can be initially discovered. However, the prevalence of changes seen around smaller craters may explain in part their shallower size frequency distribution. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Daubar, I. J.; Golombek, M. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Daubar, I. J.; Byrne, S.; McEwen, A. S.; Chojnacki, M.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Dundas, C. M.; Geissler, P.] US Geol Survey, Astrogeol Sci Ctr, 2255 N Gemini Dr, Flagstaff, AZ 86001 USA.
[Bart, G. D.] Univ Idaho, Dept Phys, 875 Perimeter Dr,MS 0903, Moscow, ID 83843 USA.
[Russell, P. S.] Natl Air & Space Museum, Smithsonian Inst, MRC 315,POB 37012, Washington, DC 20013 USA.
RP Daubar, IJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM ingrid.daubar@jpl.nasa.gov
RI Chojnacki, Matthew/A-4245-2013;
OI Chojnacki, Matthew/0000-0001-8497-8994; Dundas,
Colin/0000-0003-2343-7224
FU National Aeronautics and Space Administration
FX We are grateful for the HiRISE operations staff for acquiring and
processing the excellent data used in this study, and the CTX operations
team for discovering candidate new impact sites. Our thanks go to Rod
Heyd for answering questions about the detailed processing of HiRISE
RDRs and Guy McArthur for help with the HiView software. Patricio
Becerra also provided useful discussion. We appreciate the helpful
comments from Moses Milazzo and two anonymous reviewers, especially one
reviewer whose thoughtful and detailed comments greatly improved this
work. This work was partially supported by an appointment to the NASA
Postdoctoral Program at the Jet Propulsion Laboratory, California
Institute of Technology, administered by Oak Ridge Associated
Universities through a contract with the National Aeronautics and Space
Administration.
NR 64
TC 5
Z9 5
U1 1
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 15
PY 2016
VL 267
BP 86
EP 105
DI 10.1016/j.icarus.2015.11.032
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC3NJ
UT WOS:000369125700008
ER
PT J
AU Longobardo, A
Palomba, E
Ciarniello, M
Tosi, F
De Sanctis, MC
Capaccioni, F
Zambon, F
Ammannito, E
Filacchione, G
Raymond, CA
AF Longobardo, Andrea
Palomba, Ernesto
Ciarniello, Mauro
Tosi, Federico
De Sanctis, Maria Cristina
Capaccioni, Fabrizio
Zambon, Francesca
Ammannito, Eleonora
Filacchione, Gianrico
Raymond, Carol A.
TI Disk-resolved photometry of Vesta and Lutetia and comparison with other
asteroids
SO ICARUS
LA English
DT Article
DE Photometry; Asteroid Vesta; Asteroids, surfaces; Asteroid Eros
ID NEAR-INFRARED SPECTROSCOPY; HUBBLE-SPACE-TELESCOPE; SURFACE-COMPOSITION;
ROSETTA MISSION; BIDIRECTIONAL REFLECTANCE; IMAGING SPECTROMETER;
GALILEO PHOTOMETRY; DARK MATERIAL; DAWN MISSION; 253 MATHILDE
AB Photometry of asteroids gives fundamental information about their spectral and physical properties. The aim of this work is two-fold: (1) to calculate phase functions of Vesta and Lutetia in the visible spectral range; and (2) to compare photometric properties of all the asteroids visited by space missions, as inferred from disk-resolved photometry.
The phase functions of Vesta and Lutetia have been retrieved by performing a statistical analysis on data provided by the VIR-Dawn and the VIRTIS-Rosetta imaging spectrometers, respectively. The approach is based on the empirical procedure defined in Longobardo et al. (Longobardo, A. et al. [2014]. Icarus 240, 20-35).
The Vesta phase functions have been calculated at two wavelengths, one outside (0.75 mu m) and one inside (0.95 mu m) the pyroxene absorption band at 0.9 mu m. The steepness of the phase function at 0.75 mu m decreases from dark to bright regions, due to the increasing role of multiple scattering. Otherwise, the phase function at 0.95 mu m results in uniformity across Vesta surface, since darkening agents are spectrally featureless and their influence at wavelengths inside the pyroxene absorption band is negligible. Moreover, it is, on average, steeper than the phase functions at 0.75 mu m, due to the more important role of single scattering at 0.95 mu m.
The Lutetia phase function is instead constant across the surface due to the homogeneous spectral properties of this asteroid.
The obtained photometric curves (reflectance versus phase angle) of Vesta and Lutetia have been then compared with those retrieved in previous works on asteroids visited by space missions. Differently from comparisons of disk-integrated phase functions of asteroids performed in previous works at low phase angles (lower than 25 degrees), this work restricts to asteroid observations that are disk-resolved and occur at solar phase angles between 20 degrees and 60 degrees.
The S-type asteroids (Gaspra, Ida, Eros and Annefrank) show similar photometric curves.
The phase functions found in bright material units on Vesta are similar to those found for Steins (E-type in the Tholen taxonomy, Xe-type in the Bus one), suggesting a photometric analogy between achondritic surfaces. The latter are brighter and with a flatter phase function with respect to chondritic surfaces: we argued that this behavior is driven by optical properties of asteroid surfaces (e.g. albedo, role of multiple scattering) rather than by physical ones (e.g. grain size, roughness).
Dark material units on Vesta show an intermediate behavior between achondrites and the C-type Mathilde, confirming once again that these regions are characterized by mixtures of HED and carbonaceous chondrites.
While a clear anti-correlation is observed between reflectance and steepness of phase function for V, S and C asteroids, Lutetia shows an anomalous photometric behavior, presenting both a low reflectance and a flat phase curve, and hence cannot be grouped with other spectral classes here considered. This behavior is similar to some X-type asteroids ground-observed at low phase angles and is consistent with a chondritic composition of its surface. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Longobardo, Andrea; Palomba, Ernesto; Ciarniello, Mauro; Tosi, Federico; De Sanctis, Maria Cristina; Capaccioni, Fabrizio; Zambon, Francesca; Filacchione, Gianrico] INAF Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere, I-00133 Rome, Italy.
[Ammannito, Eleonora] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Raymond, Carol A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Longobardo, A (reprint author), INAF Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere, I-00133 Rome, Italy.
EM andrea.longobardo@iaps.inaf.it
OI Palomba, Ernesto/0000-0002-9101-6774; Tosi,
Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592
FU Italian Space Agency - ASI (Italy); Dawn Science, Instrument, and
Operations Teams; PRIN-INAF; ASI; NASA (USA)
FX VIR is funded by the Italian Space Agency - ASI (Italy) and was
developed under the leadership of INAF-Istituto di Astrofisica e
Planetologia Spaziali, Rome - Italy. The instrument was built by
Selex-Galileo, Florence-Italy. The authors acknowledge the support of
the Dawn Science, Instrument, and Operations Teams. This work was
supported by PRIN-INAF 2012, ASI and NASA (USA).
NR 86
TC 1
Z9 1
U1 0
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 15
PY 2016
VL 267
BP 204
EP 216
DI 10.1016/j.icarus.2015.12.025
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC3NJ
UT WOS:000369125700013
ER
PT J
AU Nayak, M
Nimmo, F
Udrea, B
AF Nayak, Michael
Nimmo, Francis
Udrea, Bogdan
TI Effects of mass transfer between Martian satellites on surface geology
SO ICARUS
LA English
DT Article
DE Mars; Mars, satellites; Impact processes; Cratering
ID ORBITAL EVOLUTION; IMPACT EJECTA; PHOBOS; DEIMOS; CRATER; FEATURES;
STICKNEY; GRAVITY; ORIGIN; HETEROGENEITY
AB Impacts on planetary bodies can lead to both prompt secondary craters and projectiles that reimpact the target body or nearby companions after an extended period, producing so-called "sesquinary" craters. Here we examine sesquinary cratering on the moons of Mars. We model the impact that formed Voltaire, the largest crater on the surface of Deimos, and explore the orbital evolution of resulting high-velocity ejecta across 500 years using four-body physics and particle tracking.
The bulk of mass transfer to Phobos occurs in the first 10(2) years after impact, while reaccretion of ejecta to Deimos is predicted to continue out to a 10(4) year timescale (cf. Soter, S. [1971]. Studies of the Terrestrial Planets. Cornell University). Relative orbital geometry between Phobos and Deimos plays a significant role; depending on the relative true longitude, mass transfer between the moons can change by a factor of five. Of the ejecta with a velocity range capable of reaching Phobos, 25-42% by mass reaccretes to Deimos and 12-21% impacts Phobos. Ejecta mass transferred to Mars is <10%.
We find that the characteristic impact velocity of sesquinaries on Deimos is an order of magnitude smaller than those of background (heliocentric) hypervelocity impactors and will likely result in different crater morphologies. The time-averaged flux of Deimos material to Phobos can be as high as 11% of the background (heliocentric) direct-to-Phobos impactor flux. This relatively minor contribution suggests that spectrally red terrain on Phobos (Murchie, S., Erard, S. [1996]. Icarus 123, 63-86) is not caused by Deimos material. However the high-velocity ejecta mass reaccreted to Deimos from a Voltaire-sized impact is comparable to the expected background mass accumulated on Deimos between Voltaire-size events. Considering that the high-velocity ejecta contains only 0.5% of the total mass sent into orbit, sesquinary ejecta from a Voltaire-sized impact could feasibly resurface large parts of the Moon, erasing the previous geological record. Dating the surface of Deimos may be more challenging than previously suspected. Published by Elsevier Inc.
C1 [Nayak, Michael; Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, 1156 High St, Santa Cruz, CA 95064 USA.
[Nayak, Michael] Red Sky Res LLC, 67 Northland Meadows Dr, Edgewood, NM 87105 USA.
[Udrea, Bogdan] Embry Riddle Aeronaut Univ, Dept Aerosp Engn, 600 S Clyde Morris, Daytona Beach, FL 32114 USA.
[Nayak, Michael] NASA, Ames Res Ctr, Planetary Syst Branch SST, Moffett Field, CA 94035 USA.
RP Nayak, M (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, 1156 High St, Santa Cruz, CA 95064 USA.
EM mnayak@ucsc.edu
FU Department of Defense, National Defense Science and Engineering Graduate
(NDSEG) Fellowship [32 CFR 168a]
FX This research was conducted with Government support under and awarded by
the Department of Defense, National Defense Science and Engineering
Graduate (NDSEG) Fellowship, 32 CFR 168a, with supplementary support to
M.N. provided by Red Sky Research, LLC. We gratefully acknowledge
computational support provided by Elizabeth Hyde, as well as the NASA
Ames Research Center through a contract with the University of
California Santa Cruz University Affiliated Research Center (UARC).
Thanks to Bill Folkner (JPL/Caltech) for high-fidelity long-term
Phobos/Deimos SPICE orbit propagations, and to Anthony R. Dobrovolskis
and an anonymous reviewer for insightful comments that strengthened this
manuscript. This research made use of NASA's HORIZONS
(ssd.jpl.nasa.gov), NAIF (naif.jpl.nasa.gov) and PDS (pds.nasa.gov)
databases. Opinions, interpretations and recommendations expressed are
those of the authors and are not necessarily endorsed by the US Air
Force or the Department of Defense.
NR 79
TC 2
Z9 2
U1 2
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 15
PY 2016
VL 267
BP 220
EP 231
DI 10.1016/j.icarus.2015.12.026
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC3NJ
UT WOS:000369125700015
ER
PT J
AU Polishook, D
Moskovitz, N
Binzel, RP
Burt, B
DeMeo, FE
Hinkle, ML
Lockhart, M
Mommert, M
Person, M
Thirouin, A
Thomas, CA
Trilling, D
Willman, M
Aharonson, O
AF Polishook, D.
Moskovitz, N.
Binzel, R. P.
Burt, B.
DeMeo, F. E.
Hinkle, M. L.
Lockhart, M.
Mommert, M.
Person, M.
Thirouin, A.
Thomas, C. A.
Trilling, D.
Willman, M.
Aharonson, O.
TI A 2 km-size asteroid challenging the rubble-pile spin barrier - A case
for cohesion
SO ICARUS
LA English
DT Article
DE Asteroids; Asteroids, rotation; Rotational dynamics; Photometry
ID NEAR-EARTH ASTEROIDS; MAIN BELT ASTEROIDS; 29075 1950 DA;
PHYSICAL-PROPERTIES; ROTATIONAL BREAKUP; BINARY ASTEROIDS; P/2013 R3;
DISRUPTION; ORIGIN; REGOLITH
AB The rubble pile spin barrier is an upper limit on the rotation rate of asteroids larger than similar to 200-300 m. Among thousands of asteroids with diameters larger than similar to 300 m, only a handful of asteroids are known to rotate faster than 2.0 h, all are in the sub-km range (<= 0.6 km). Here we present photometric measurements suggesting that (60716) 2000 GD65, an S-complex, inner-main belt asteroid with a relatively large diameter of 2.3(-0.7)(+0.6) km, completes one rotation in 1.9529 +/- 0.0002 h. Its unique diameter and rotation period allow us to examine scenarios about asteroid internal structure and evolution: a rubble pile bound only by gravity; a rubble-pile with strong cohesion; a monolithic structure; an asteroid experiencing mass shedding; an asteroid experiencing YORP spin-up/down; and an asteroid with a unique octahedron shape results with a four-peak lightcurve and a 3.9 h period. We find that the most likely scenario includes a lunar-like cohesion that can prevent (60716) 2000 GD65 from disrupting without requiring a monolithic structure or a unique shape. Due to the uniqueness of (60716)2000 GD65, we suggest that most asteroids typically have smaller cohesion than that of lunar regolith. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Polishook, D.; Aharonson, O.] Weizmann Inst Sci, Dept Earth & Planetary Sci, IL-7610001 Rehovot, Israel.
[Moskovitz, N.; Hinkle, M. L.; Thirouin, A.] Lowell Observ, 1400 West Mars Hill Rd, Flagstaff, AZ 86001 USA.
[Binzel, R. P.; Burt, B.; DeMeo, F. E.; Person, M.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Lockhart, M.] POB 391274, Cambridge, MA 02139 USA.
[Mommert, M.; Trilling, D.] No Arizona Univ, Dept Phys & Astron, POB 6010, Flagstaff, AZ 86011 USA.
[Thomas, C. A.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Thomas, C. A.] Oak Ridge Associated Univ, NASA Postdoctoral Program, POB 117,MS 36, Oak Ridge, TN 37831 USA.
[Thomas, C. A.] Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
[Trilling, D.] S African Astron Observ, Cape Town, South Africa.
[Trilling, D.] Univ Western Cape, ZA-7535 Bellville, South Africa.
[Willman, M.] Univ Hawaii, Inst Astrophys, Honolulu, HI 96822 USA.
RP Polishook, D (reprint author), Weizmann Inst Sci, Dept Earth & Planetary Sci, IL-7610001 Rehovot, Israel.
FU Ministry of Science, Technology and Space of the Israeli government; AXA
Research Fund; NASA [NNX12AL26G]; NASA; Helen Kimmel Center for
Planetary Science; ISF I-CORE program "Origins: From the Big Bang to
Planets"; NASA NEOO Grant [NNX14AN82G]
FX We are grateful to the referees for their thorough reports that improve
the manuscript. We thank William Bottke and Dave O'Brien for their
insights and fruitful discussion. DP is grateful to the Ministry of
Science, Technology and Space of the Israeli government for their Ramon
fellowship for post-docs, and the AXA Research Fund for their generous
post-doc fellowship, during the years of observations and analysis. FED
acknowledges funding from NASA under Grant No. NNX12AL26G. CAT was
supported by an appointment to the NASA Postdoctoral Program at Goddard
Space Flight Center, administrated by Oak Ridge Associated Universities
through a contract with NASA. OA would like to acknowledge support from
the Helen Kimmel Center for Planetary Science and the ISF I-CORE program
"Origins: From the Big Bang to Planets".; We acknowledge support from
NASA NEOO Grant No. NNX14AN82G, awarded to the Mission Accessible
Near-Earth Object Survey (MANOS). We are thankful to the Wise
Observatory staff for their continuous help and generous time
allocation. Observations for this study were performed in Arizona,
Chile, Hawaii and Israel. The people of all nations that support hosting
professional observatories are praised for understanding and supporting
the importance of astronomical studies.
NR 79
TC 2
Z9 2
U1 0
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 15
PY 2016
VL 267
BP 243
EP 254
DI 10.1016/j.icarus.2015.12.031
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC3NJ
UT WOS:000369125700017
ER
PT J
AU Pravec, P
Scheirich, P
Kusnirak, P
Hornoch, K
Galad, A
Naidu, SP
Pray, DP
Vilagi, J
Gajdos, S
Kornos, L
Krugly, YN
Cooney, WR
Gross, J
Terrell, D
Gaftonyuk, N
Pollock, J
Husarik, M
Chiorny, V
Stephens, RD
Durkee, R
Reddy, V
Dyvig, R
Vrastil, J
Zizka, J
Mottola, S
Hellmich, S
Oey, J
Benishek, V
Kryszczynska, A
Higgins, D
Ries, J
Marchis, F
Baek, M
Macomber, B
Inasaridze, R
Kvaratskhelia, O
Ayvazian, V
Rumyantsev, V
Masi, G
Colas, F
Lecacheux, J
Montaigut, R
Leroy, A
Brown, P
Krzeminski, Z
Molotov, I
Reichart, D
Haislip, J
LaCluyze, A
AF Pravec, P.
Scheirich, P.
Kusnirak, P.
Hornoch, K.
Galad, A.
Naidu, S. P.
Pray, D. P.
Vilagi, J.
Gajdos, S.
Kornos, L.
Krugly, Yu. N.
Cooney, W. R.
Gross, J.
Terrell, D.
Gaftonyuk, N.
Pollock, J.
Husarik, M.
Chiorny, V.
Stephens, R. D.
Durkee, R.
Reddy, V.
Dyvig, R.
Vrastil, J.
Zizka, J.
Mottola, S.
Hellmich, S.
Oey, J.
Benishek, V.
Kryszczynska, A.
Higgins, D.
Ries, J.
Marchis, F.
Baek, M.
Macomber, B.
Inasaridze, R.
Kvaratskhelia, O.
Ayvazian, V.
Rumyantsev, V.
Masi, G.
Colas, F.
Lecacheux, J.
Montaigut, R.
Leroy, A.
Brown, P.
Krzeminski, Z.
Molotov, I.
Reichart, D.
Haislip, J.
LaCluyze, A.
TI Binary asteroid population. 3. Secondary rotations and elongations
SO ICARUS
LA English
DT Article
DE Asteroids, rotation; Asteroids, dynamics; Near-Earth objects; Photometry
ID RUBBLE-PILE SATELLITES; 2001 SN263; 1994 CC; EVOLUTION; RADAR;
LIGHTCURVES; ORIGIN; PAIRS
AB We collected data on rotations and elongations of 46 secondaries of binary and triple systems among near-Earth, Mars-crossing and small main belt asteroids. 24 were found or are strongly suspected to be synchronous (in 1:1 spin-orbit resonance), and the other 22, generally on more distant and/or eccentric orbits, were found or are suggested to have asynchronous rotations. For 18 of the synchronous secondaries, we constrained their librational angles, finding that their long axes pointed to within 20 degrees of the primary on most epochs. The observed anti-correlation of secondary synchroneity with orbital eccentricity and the limited librational angles agree with the theories by Cuk and Nesvorny (Cuk, M., Nesvorny, D. [2010]. Icarus 207, 732-743) and Naidu and Margot (Naidu, S.P., Margot, J.-L. [2015]. Astron. J. 149, 80). A reason for the asynchronous secondaries being on wider orbits than synchronous ones may be longer tidal circularization time scales at larger semi-major axes. The asynchronous secondaries show relatively fast spins; their rotation periods are typically < 10 h. An intriguing observation is a paucity of chaotic secondary rotations; with an exception of (35107) 1991 VH, the secondary rotations are single-periodic with no signs of chaotic rotation and their periods are constant on timescales from weeks to years. The secondary equatorial elongations show an upper limit of a(2)/b(2)similar to 1.5. The lack of synchronous secondaries with greater elongations appears consistent, considering uncertainties of the axis ratio estimates, with the theory by Cuk and Nesvorny that predicts large regions of chaotic rotation in the phase space for a(2)/b(2) >= root 2. Alternatively, secondaries may not form or stay very elongated in gravitational (tidal) field of the primary. It could be due to the secondary fission mechanism suggested by Jacobson and Scheeres (Jacobson, S.A., Scheeres, D.J. [2011]. Icarus 214, 161-178), as its efficiency is correlated with the secondary elongation. Sharma (Sharma, I. [2014]. Icarus 229, 278-294) found that rubble-pile satellites with a(2)/b(2) less than or similar to 1.5 are more stable to finite structural perturbations than more elongated ones. It appears that more elongated secondaries, if they originally formed in spin fission of parent asteroid, are less likely to survive intact and they more frequently fail or fission. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Pravec, P.; Scheirich, P.; Kusnirak, P.; Hornoch, K.; Galad, A.; Vrastil, J.] Acad Sci Czech Republic, Astron Inst, Fricova 1, CZ-25165 Ondrejov, Czech Republic.
[Galad, A.; Vilagi, J.; Gajdos, S.; Kornos, L.] FMPI UK, Dept Astron Phys Earth & Meteorol, Modra Observ, SK-84248 Bratislava, Slovakia.
[Naidu, S. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Pray, D. P.] Sugarloaf Mt Observ, South Deerfield, MA 01373 USA.
[Krugly, Yu. N.; Chiorny, V.] Kharkov Natl Univ, Inst Astron, Sumska Str 35, UA-61022 Kharkov, Ukraine.
[Cooney, W. R.; Gross, J.; Terrell, D.] Sonoita Res Observ, 77 Paint Trail, Sonoita, AZ 85637 USA.
[Terrell, D.] Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Gaftonyuk, N.] Crimean Astrophys Observ, Dept Radioastron & Geodynam, Simeiz 98680, Crimea, Ukraine.
[Pollock, J.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA.
[Husarik, M.] Slovak Acad Sci, Astron Inst, SK-05960 Tatranska Lomnica, Slovakia.
[Stephens, R. D.] Ctr Solar Syst Studies, 9302 Pittsburgh Ave,Suite 200, Rancho Cucamonga, CA 91730 USA.
[Durkee, R.] Shed Sci Observ, 5213 Washburn Ave S, Minneapolis, MN 55410 USA.
[Reddy, V.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Dyvig, R.] Badlands Observ, 12 Ash St,POB 37, Quinn, SD 57775 USA.
[Vrastil, J.; Zizka, J.] Charles Univ Prague, Fac Math & Phys, Inst Astron, V Holesovickach 2, CZ-18000 Prague 8, Czech Republic.
[Mottola, S.; Hellmich, S.] German Aerosp Ctr DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany.
[Oey, J.] Blue Mt Observ, Leura, NSW, Australia.
[Benishek, V.] Belgrade Astron Observ, Volgina 7, Belgrade 11060 38, Serbia.
[Kryszczynska, A.] Adam Mickiewicz Univ, Fac Phys, Astron Observ Inst, Sloneczna 36, PL-60286 Poznan, Poland.
[Higgins, D.] Hunters Hill Observ, Canberra, ACT, Australia.
[Ries, J.] Univ Texas Austin, Dept Astron, McDonald Observ, 1 Univ Stn C1400, Austin, TX 78712 USA.
[Marchis, F.; Baek, M.] SETI Inst, Carl Sagan Ctr, 189 Bernado Ave, Mountain View, CA 94043 USA.
[Macomber, B.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Inasaridze, R.; Kvaratskhelia, O.; Ayvazian, V.] Ilia State Univ, Kharadze Abastumani Astrophys Observ, G Tsereteli Str 3, Tbilisi 0162, Rep of Georgia.
[Rumyantsev, V.] Crimean Astrophys Observ, Nauchnyi 98409, Crimea, Ukraine.
[Masi, G.] Campo Catino Observ, I-03016 Guarcino, Italy.
[Masi, G.] Virtual Telescope Project, I-03023 Ceccano, Italy.
[Colas, F.; Lecacheux, J.] Observ Paris, CNRS, IMCCE, 77 Ave Denfert Rochereau, F-75014 Paris, France.
[Montaigut, R.; Leroy, A.] OPERA Observ, F-33820 St Palais, France.
[Brown, P.; Krzeminski, Z.] Univ Western Ontario, Dept Phys & Astron, Elginfield Observ, London, ON N6A 3K7, Canada.
[Molotov, I.] Russian Acad Sci, Keldysh Inst Appl Math, Miusskaya Sq 4, Moscow 125047, Russia.
[Reichart, D.; Haislip, J.; LaCluyze, A.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27514 USA.
RP Pravec, P (reprint author), Acad Sci Czech Republic, Astron Inst, Fricova 1, CZ-25165 Ondrejov, Czech Republic.
RI Baek, Minjin/L-4425-2016; Pravec, Petr/G-9037-2014; Scheirich,
Peter/H-4331-2014; Galad, Adrian/G-9011-2014;
OI Baek, Minjin/0000-0002-9698-2525; Scheirich, Peter/0000-0001-8518-9532;
Rumyantsev, Vasilij/0000-0003-1894-7019
FU Grant Agency of the Czech Republic [P209/12/0229, 15-07193S]; Slovak
Grant Agency for Science VEGA [1/0670/13, 2/0032/14]; Gene Shoemaker NEO
grant from the Planetary Society; project ITMS - European Regional
Development Fund [26220120009]; NASA [NNX11AD62G, NNX14AJ80G]; Shota
Rustaveli National Science Foundation [FR/379/6-300/14]
FX We thank to Alan Harris, Seth Jacobson, Michael Efroimsky, Matija Cuk,
Ishan Sharma and Masatoshi Hirabayashi for fruitful discussions on a
number of things in this paper. The work at Ondrejov and observations
with the Danish 1.54-m telescope on the ESO La Silla station were
supported by the Grant Agency of the Czech Republic, Grants P209/12/0229
and 15-07193S. The work at Modra was supported by the Slovak Grant
Agency for Science VEGA, Grant 1/0670/13. Operations at Sugarloaf
Mountain were supported by a Gene Shoemaker NEO grant from the Planetary
Society. The work at Tatranska Lomnica was supported by the Slovak Grant
Agency for Science VEGA, Grant 2/0032/14 and project ITMS No.
26220120009, based on the supporting operational Research and
development program financed from the European Regional Development
Fund. The work at SETI Institute was supported by NASA Grants NNX11AD62G
and NNX14AJ80G. The work at Abastumani was supported by the Shota
Rustaveli National Science Foundation, Grant FR/379/6-300/14. We thank
to S. Nudds for her contribution with observations from Elginfield
Observatory, University of Western Ontario.
NR 75
TC 3
Z9 3
U1 3
U2 8
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 15
PY 2016
VL 267
BP 267
EP 295
DI 10.1016/j.icarus.2015.12.019
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC3NJ
UT WOS:000369125700019
ER
PT J
AU Pilorget, C
Fernando, J
Ehlmann, BL
Schmidt, F
Hiroi, T
AF Pilorget, C.
Fernando, J.
Ehlmann, B. L.
Schmidt, F.
Hiroi, T.
TI Wavelength dependence of scattering properties in the VIS-NIR and links
with grain-scale physical and compositional properties
SO ICARUS
LA English
DT Article
DE Photometry; Radiative transfer; Regoliths; Terrestrial planets
ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; LIGHT-SCATTERING; PHOTOMETRIC
PROPERTIES; PARTICULATE SURFACES; MULTIPLE-SCATTERING; GALILEO
PHOTOMETRY; PLANETARY SURFACE; MERIDIANI PLANUM; INVERSE PROBLEMS; GUSEV
CRATER
AB Surface scattered sunlight carries important information about the composition and microtexture of surface materials, thus enabling tracing back the geological and climatic processes that occurred on the planetary body. Here we perform laboratory spectro-goniometric measurements of granular samples (45-75 mu m fraction) with different composition and physical properties over the VIS-NIR spectral range (0.4-2.5 mu m). To quantify the evolution of the scattering properties over the VIS-NIR, we use an inversion procedure based on a Bayesian approach to estimate photometric parameters from the Hapke radiative transfer model. The granular samples are also carefully characterized by optical and SEM techniques in order to link these scattering variations with the grains' physical properties. Results show that the scattering properties are wavelength-dependent and can vary significantly over the VIS-NIR spectral range. In particular, the phase function of a granular material is affected by both the absorptivity and the external and internal structure of the grains, from the millimeter scale down to the wavelength scale. Our results also confirm that the macroscopic roughness parameter, as defined by Hapke, is to first order correlated with the absorptivity of the particles, through multiple scattering effects, and thus mostly corresponds to a measurement of the particles shadowing. Photometric datasets, typically obtained at a given wavelength that can vary from one study to another, should therefore be compared and interpreted with caution when extrapolating across wavelengths. Our results also suggest that multi-wavelength photometry could potentially provide a much richer signature than with single-wavelength photometry, opening new perspectives into the characterization of surface materials. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Pilorget, C.; Ehlmann, B. L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Pilorget, C.] CNRS Univ Paris Sud, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France.
[Fernando, J.; Schmidt, F.] Univ Paris 11, GEOPS, UMR8148, F-91405 Orsay, France.
[Fernando, J.; Schmidt, F.] CNRS, F-91405 Orsay, France.
[Ehlmann, B. L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Hiroi, T.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
RP Pilorget, C (reprint author), CNRS Univ Paris Sud, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France.
EM cedric.pilorget@ias.u-psud.fr
FU CNES; European Research Council under the European Unions Seventh
Framework Program [280168]; Institut National des Sciences de l'Univers
(INSU); Centre National de la Recherche Scientifique (CNRS); Centre
National d'Etude Spatiale (CNES) through the Programme National de
Planetologie; NASA; NASA SSERVI program; [NNX14AG54G]
FX We would like to thank all our colleagues at Caltech and GEOPS for
inspiration and advice, in particular Chi Ma and George Ross man for
their invaluable help in the sample characterization. CP and BE
acknowledge partial support from NNX14AG54G. CP also acknowledges
support from CNES and JF support from the European Research Council
under the European Unions Seventh Framework Program (FP7/2007-2013)/ERC
Grant Agreement No. 280168. SF and JF acknowledge support from the
Institut National des Sciences de l'Univers (INSU), the Centre National
de la Recherche Scientifique (CNRS) and Centre National d'Etude Spatiale
(CNES) through the Programme National de Planetologie. RELAB is a
multiuser facility supported by NASA. TH was partially supported by NASA
SSERVI program.
NR 53
TC 1
Z9 1
U1 1
U2 7
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAR 15
PY 2016
VL 267
BP 296
EP 314
DI 10.1016/j.icarus.2015.12.029
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DC3NJ
UT WOS:000369125700020
ER
PT J
AU Kim, K
Park, C
Kwon, D
Kim, D
Meyyappan, M
Jeon, S
Lee, JS
AF Kim, Kihyun
Park, Chanoh
Kwon, Donghoon
Kim, Donghoon
Meyyappan, M.
Jeon, Sangmin
Lee, Jeong-Soo
TI Silicon nanowire biosensors for detection of cardiac troponin I (cTnI)
with high sensitivity
SO BIOSENSORS & BIOELECTRONICS
LA English
DT Article
DE Honeycomb nanowire; Field-effect transistor; Biosensor; Cardiac troponin
I; Limit of detection; Debye length
ID ACUTE MYOCARDIAL-INFARCTION; LABEL-FREE DETECTION; ANODIC-STRIPPING
VOLTAMMETRY; EFFECT TRANSISTOR SENSORS; CARBON-PASTE ELECTRODE;
ELECTRICAL DETECTION; DIAGNOSIS; IMMUNODETECTION; NANOSENSORS; MARKERS
AB We have demonstrated highly sensitive and label-free detection of cardiac troponin I (cTnI), a biomarker for diagnosis of acute myocardial infarction, using silicon nanowire field-effect transistors. A honeycomb-like structure is utilized for nanowire configuration to offer improved electrical performance and increased sensing area. The fabricated devices show n-type behavior with a relatively high ON-OFF current ratio, small sub-threshold swing and low gate leakage current. Monoclonal antibodies for cTnI were covalently immobilized on the nanowire surface and the attachment of antibodies is clearly visualized by atomic force microscope. The sensitivity with various concentrations of buffer solution was also investigated in order to determine the optimal buffer condition. The devices exhibit highest sensitivity under buffer solutions with low ion concentration. In addition, the detection limit of the sensor is as low as similar to 5 pg/mL, the lowest reported in the literature to date and nearly an order of magnitude smaller than the suggested threshold limit. The fabricated devices demonstrate a good selectivity for detecting cTnI. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Kim, Kihyun; Meyyappan, M.] Pohang Univ Sci & Technol POSTECH, Dept Creat IT Engn, Pohang 37673, South Korea.
[Kim, Kihyun; Meyyappan, M.] Pohang Univ Sci & Technol POSTECH, Future IT Innovat Lab, Pohang 37673, South Korea.
[Park, Chanoh; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang 37673, South Korea.
[Kwon, Donghoon; Jeon, Sangmin] Pohang Univ Sci & Technol POSTECH, Dept Chem Engn, Pohang 37673, South Korea.
[Kim, Donghoon; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Dept Elect Engn, Pohang 37673, South Korea.
[Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lee, JS (reprint author), Pohang Univ Sci & Technol POSTECH, Dept Elect Engn, Pohang 37673, South Korea.
EM ljs6951@postech.ac.kr
FU MSIP (Ministry of Science, ICT and Future Planning), Republic of Korea,
under the "ICT Consilience Creative Program" [IITP-2015-R0346-15-1007];
Agency for Defense Development, Republic of Korea [ADD-14-02-06-20]
FX This work was supported by the MSIP (Ministry of Science, ICT and Future
Planning), Republic of Korea, under the "ICT Consilience Creative
Program" (IITP-2015-R0346-15-1007) supervised by the IITP (Institute for
Information & communications Technology Promotion), and by the Agency
for Defense Development (ADD-14-02-06-20), Republic of Korea.
NR 35
TC 12
Z9 12
U1 20
U2 97
PU ELSEVIER ADVANCED TECHNOLOGY
PI OXFORD
PA OXFORD FULFILLMENT CENTRE THE BOULEVARD, LANGFORD LANE, KIDLINGTON,
OXFORD OX5 1GB, OXON, ENGLAND
SN 0956-5663
EI 1873-4235
J9 BIOSENS BIOELECTRON
JI Biosens. Bioelectron.
PD MAR 15
PY 2016
VL 77
BP 695
EP 701
DI 10.1016/j.bios.2015.10.008
PG 7
WC Biophysics; Biotechnology & Applied Microbiology; Chemistry, Analytical;
Electrochemistry; Nanoscience & Nanotechnology
SC Biophysics; Biotechnology & Applied Microbiology; Chemistry;
Electrochemistry; Science & Technology - Other Topics
GA CZ0AG
UT WOS:000366766900100
ER
PT J
AU Tokgoz, C
Dardona, S
Soldner, NC
Wheeler, KR
AF Tokgoz, Cagatay
Dardona, Sameh
Soldner, Nicholas C.
Wheeler, Kevin R.
TI Modeling and characterization of partially inserted electrical connector
faults
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID DOMAIN REFLECTOMETRY; WIRING FAULTS; LOCATION
AB Faults within electrical connectors are prominent in avionics systems due to improper installation, corrosion, aging, and strained harnesses. These faults usually start off as undetectable with existing inspection techniques and increase in magnitude during the component lifetime. Detection and modeling of these faults are significantly more challenging than hard failures such as open and short circuits. Hence, enabling the capability to locate and characterize the precursors of these faults is critical for timely preventive maintenance and mitigation well before hard failures occur. In this paper, an electrical connector model based on a two-level nonlinear least squares approach is proposed. The connector is first characterized as a transmission line, broken into key components such as the pin, socket, and connector halves. Then, the fact that the resonance frequencies of the connector shift as insertion depth changes from a fully inserted to a barely touching contact is exploited. The model precisely captures these shifts by varying only two length parameters. It is demonstrated that the model accurately characterizes a partially inserted connector. (C) 2016 AIP Publishing LLC.
C1 [Tokgoz, Cagatay; Dardona, Sameh; Soldner, Nicholas C.] United Technol Res Ctr, E Hartford, CT 06118 USA.
[Wheeler, Kevin R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Tokgoz, C (reprint author), United Technol Res Ctr, E Hartford, CT 06118 USA.
EM tokgozc@utrc.utc.com
RI Tokgoz, Cagatay/N-1353-2016
OI Tokgoz, Cagatay/0000-0003-4664-0444
FU NASA Ames Research Center [NNA12AB91C]
FX The authors gratefully acknowledge the NASA Ames Research Center for
their support under Contract No. NNA12AB91C. The authors would like to
thank Dr. Stefan Schuet and Dr. Dogan Timucin, NASA Ames Research
Center, for their useful comments and suggestions.
NR 16
TC 2
Z9 2
U1 1
U2 6
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-8979
EI 1089-7550
J9 J APPL PHYS
JI J. Appl. Phys.
PD MAR 14
PY 2016
VL 119
IS 10
AR 104501
DI 10.1063/1.4943178
PG 7
WC Physics, Applied
SC Physics
GA DH7MA
UT WOS:000372976900020
ER
PT J
AU Jiang, Z
Caves, CM
AF Jiang, Zhang
Caves, Carlton M.
TI Particle-number-conserving Bogoliubov approximation for Bose-Einstein
condensates using extended catalytic states
SO PHYSICAL REVIEW A
LA English
DT Article
ID 2-PHOTON QUANTUM OPTICS; GROSS-PITAEVSKII; ENTANGLEMENT; PHASE; GAS;
FORMALISM; VALIDITY; DYNAMICS; LIMITS; TRAP
AB We encode the many-body wave function of a Bose-Einstein condensate (BEC) in the N-particle sector of an extended catalytic state. This catalytic state is a coherent state for the condensate mode and an arbitrary state for the modes orthogonal to the condensate mode. Going to a time-dependent interaction picture where the state of the condensate mode is displaced to the vacuum, we can organize the effective Hamiltonian by powers of N-1/2. Requiring the terms of order N-1/2 to vanish gives the Gross-Pitaevskii equation. Going to the next order, N-0, we derive equations for the number-conserving Bogoliubov approximation, first given by Castin and Dum [Phys. Rev. A 57, 3008 (1998)]. In contrast to other approaches, ours is well suited to calculating the state evolution in the Schrodinger picture; moreover, it is straightforward to generalize our method to multicomponent BECs and to higher-order corrections.
C1 [Jiang, Zhang; Caves, Carlton M.] Univ New Mexico, Ctr Quantum Informat & Control, MSC07-4220, Albuquerque, NM 87131 USA.
[Jiang, Zhang] NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab QuAIL, Mail Stop 269-1, Moffett Field, CA 94035 USA.
[Jiang, Zhang] Stinger Ghaffarian Technol Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA.
[Caves, Carlton M.] Univ Queensland, Sch Math & Phys, Ctr Engineered Quantum Syst, Brisbane, Qld 4072, Australia.
RP Jiang, Z; Caves, CM (reprint author), Univ New Mexico, Ctr Quantum Informat & Control, MSC07-4220, Albuquerque, NM 87131 USA.; Jiang, Z (reprint author), NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab QuAIL, Mail Stop 269-1, Moffett Field, CA 94035 USA.; Jiang, Z (reprint author), Stinger Ghaffarian Technol Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA.; Caves, CM (reprint author), Univ Queensland, Sch Math & Phys, Ctr Engineered Quantum Syst, Brisbane, Qld 4072, Australia.
EM zhang.jiang@nasa.gov; ccaves@unm.edu
RI Caves, Carlton/K-8167-2014
OI Caves, Carlton/0000-0001-8876-1186
FU National Science Foundation [PHY-1212445, PHY-1314763]; Office of Naval
Research Grant [N00014-15-1-2167]
FX The authors thanks A. B. Tacla for useful and stimulating conversations.
This work was supported in part by National Science Foundation Grants
No. PHY-1212445 and No. PHY-1314763 and by Office of Naval Research
Grant No. N00014-15-1-2167.
NR 49
TC 0
Z9 0
U1 2
U2 4
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD MAR 14
PY 2016
VL 93
IS 3
AR 033623
DI 10.1103/PhysRevA.93.033623
PG 18
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA DG9JJ
UT WOS:000372398300010
ER
PT J
AU Richard, S
Nelson, RP
Umurhan, OM
AF Richard, Samuel
Nelson, Richard P.
Umurhan, Orkan M.
TI Vortex formation in protoplanetary discs induced by the vertical shear
instability
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; hydrodynamics; instabilities; turbulence;
protoplanetary discs
ID ROSSBY-WAVE INSTABILITY; BAROCLINIC VORTICITY PRODUCTION; THIN ACCRETION
DISKS; DEAD-ZONES; CONVECTIVE OVERSTABILITY; CIRCUMSTELLAR DISKS;
LINEAR-ANALYSIS; GIANT PLANET; ZONAL FLOWS; TURBULENCE
AB We present the results of 2D and 3D hydrodynamic simulations of idealized protoplanetary discs that examine the formation and evolution of vortices by the vertical shear instability (VSI). In agreement with recent work, we find that discs with radially decreasing temperature profiles and short thermal relaxation time-scales, are subject to the axisymmetric VSI. In three dimensions, the resulting velocity perturbations give rise to quasi-axisymmetric potential vorticity perturbations that break up into discrete vortices, in a manner that is reminiscent of the Rossby wave instability. Discs with very short thermal evolution time-scales (i.e. tau <= 0.1 local orbit periods) develop strong vorticity perturbations that roll up into vortices that have small aspect ratios (chi <= 2) and short lifetimes (similar to a few orbits). Longer thermal time-scales give rise to vortices with larger aspect ratios (6 <= chi <= 10), and lifetimes that depend on the entropy gradient. A steeply decreasing entropy profile leads to vortex lifetimes that exceed the simulation run times of hundreds of orbital periods. Vortex lifetimes in discs with positive or weakly decreasing entropy profiles are much shorter, being 10s of orbits at most, suggesting that the subcritical baroclinic instability plays an important role in sustaining vortices against destruction through the elliptical instability. Applied to the outer regions of protoplanetary discs, where the VSI is most likely to occur, our results suggest that vortices formed by the VSI are likely to be short-lived structures.
C1 [Richard, Samuel; Nelson, Richard P.] Queen Mary Univ London, Astron Unit, Mile End Rd, London E1 4NS, England.
[Umurhan, Orkan M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Umurhan, Orkan M.] SETI Inst, 189 Bernardo Way, Mountain View, CA 94043 USA.
RP Richard, S (reprint author), Queen Mary Univ London, Astron Unit, Mile End Rd, London E1 4NS, England.; Umurhan, OM (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.; Umurhan, OM (reprint author), SETI Inst, 189 Bernardo Way, Mountain View, CA 94043 USA.
EM samuel.richard@qmul.ac.uk; orkan.m.umurhan@nasa.gov
FU BIS National E-Infrastructure capital grant [ST/K000373/1]; STFC
Operations grant [ST/K0003259/1]
FX This work used the DiRAC Complexity system, operated by the University
of Leicester IT Services, which forms part of the STFC DiRAC HPC
Facility (www.dirac.ac.uk). The equipment is funded by BIS National
E-Infrastructure capital grant ST/K000373/1 and STFC Operations grant
ST/K0003259/1. DiRAC is part of the national E-Infrastructure.
NR 52
TC 4
Z9 4
U1 2
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 11
PY 2016
VL 456
IS 4
BP 3571
EP 3584
DI 10.1093/mnras/stv2898
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LM
UT WOS:000372265800012
ER
PT J
AU Del Santo, M
Belloni, TM
Tomsick, JA
Sbarufatti, B
Bel, MC
Casella, P
Castro-Tirado, A
Corbel, S
Grinberg, V
Homan, J
Kalemci, E
Motta, S
Munoz-Darias, T
Pottschmidt, K
Rodriguez, J
Wilms, J
AF Del Santo, M.
Belloni, T. M.
Tomsick, J. A.
Sbarufatti, B.
Bel, M. Cadolle
Casella, P.
Castro-Tirado, A.
Corbel, S.
Grinberg, V.
Homan, J.
Kalemci, E.
Motta, S.
Munoz-Darias, T.
Pottschmidt, K.
Rodriguez, J.
Wilms, J.
TI Spectral and timing evolution of the bright failed outburst of the
transient black hole Swift J174510.8-262411
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; radiation mechanisms:
non-thermal; stars: individual: Swift J174510.8-262411; Gamma-rays:
general; X-rays: binaries
ID X-RAY BINARIES; QUASI-PERIODIC OSCILLATIONS; LOW-HARD STATE; GX 339-4;
CYGNUS X-1; LOW/HARD STATE; ACCRETION DISK; XTE J1550-564; SOFT STATE;
VARIABILITY
AB We studied time variability and spectral evolution of the Galactic black hole transient Swift J174510.8-262411 during the first phase of its outburst. INTEGRAL and Swift observations collected from 2012 September 16 until October 30 have been used. The total squared fractional rms values did not drop below 5 per cent and quasi-periodic oscillations (QPOs), when present, were type-C, indicating that the source never made the transition to the soft-intermediate state. Even though the source was very bright (up to 1 Crab in hard X-rays), it showed a so called failed outburst as it never reached the soft state. XRT and IBIS broad-band spectra, well represented by a hybrid thermal/non-thermal Comptonization model, showed physical parameters characteristic of the hard and intermediate states. In particular, the derived temperature of the geometrically thin disc blackbody was about 0.6 keV at maximum. We found a clear decline of the optical depth of the corona electrons (close to values of 0.1), as well as of the total compactness ratio l(h)/l(s). The hard-to-hard/intermediate state spectral transition is mainly driven by the increase in the soft photon flux in the corona, rather than small variations of the electron heating. This, associated with the increasing of the disc temperature, is consistent with a disc moving towards the compact object scenario, i.e. the truncated-disc model. Moreover, this scenario is consistent with the decreasing fractional squared rms and increasing of the noise and QPO frequency. In our final group of observations, we found that the contribution from the non-thermal Comptonization to the total power supplied to the plasma is 0.59(-0.05)(+0.02) and that the thermal electrons cool to kT(e) < 26 keV.
C1 [Del Santo, M.] IASF Palermo, Ist Nazl Astrofis, Via Ugo La Malfa 153, I-90146 Palermo, Italy.
[Belloni, T. M.; Sbarufatti, B.] Osserv Astron Brera, Ist Nazl Astrofis, Via E Bianchi 46, I-23807 Merate, Italy.
[Tomsick, J. A.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
[Sbarufatti, B.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Bel, M. Cadolle] Max Planck Comp & Data Facil, D-85748 Garching, Germany.
[Casella, P.] Osserv Astron Roma, Ist Nazl Astrofis, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
[Castro-Tirado, A.] CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain.
[Corbel, S.; Wilms, J.] Univ Paris Diderot, CEA CNRS, CEA DSM IRFU SAp, Lab AIM,UMR 7158, F-91191 Gif Sur Yvette, France.
[Grinberg, V.; Homan, J.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave 37-582D, Cambridge, MA 02139 USA.
[Homan, J.] SRON Netherlands Inst Space Res, SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
[Kalemci, E.] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey.
[Motta, S.] Univ Oxford, Astrophys, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
[Munoz-Darias, T.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Munoz-Darias, T.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Pottschmidt, K.] Univ Maryland Baltimore Cty, CRESST, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA.
[Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, Sternwartstr 7, D-96049 Bamberg, Germany.
RP Del Santo, M (reprint author), IASF Palermo, Ist Nazl Astrofis, Via Ugo La Malfa 153, I-90146 Palermo, Italy.; Belloni, TM (reprint author), Osserv Astron Brera, Ist Nazl Astrofis, Via E Bianchi 46, I-23807 Merate, Italy.; Tomsick, JA (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM melania@ifc.inaf.it; tomaso.belloni@brera.inaf.it;
jtomsick@ssl.berkeley.edu
RI Wilms, Joern/C-8116-2013;
OI Wilms, Joern/0000-0003-2065-5410; Sbarufatti, Boris/0000-0001-6620-8347
FU INAF PRIN; NASA [NNX13AJ81G, NNX14AC56G, NAS8-03060]; NASA through the
Smithsonian Astrophysical Observatory (SAO) [SV3-73016]; French Research
National Agency: CHAOS project [ANR-12-BS05-0009]; UnivEarthS Labex
programme of Sorbonne Paris Cite [ANR-10-LABX-0023,
ANR-11-IDEX-0005-02]; Spanish Ministerio de Economia y competitividad
(MINECO) [AYA2013-42627]; ESA Denmark; ESA France; ESA Germany; ESA
Italy; ESA Switzerland; ESA Spain; ESA Poland; ESA Russia; ESA USA
FX MDS thanks Milvia Capalbi and Carlo Ferrigno for useful discussion on
Swift/XRT and INTEGRAL data analysis, respectively. TMB acknowledges
support from INAF PRIN 2012-6. JAT acknowledges partial support from the
Swift Guest Observer programme through NASA grants NNX13AJ81G and
NNX14AC56G. VG acknowledges funding support by NASA through the
Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT
for Support of the Chandra X-Ray Center (CXC) and Science Instruments;
CXC is operated by SAO for and on behalf of NASA under contract
NAS8-03060. JR acknowledges funding support from the French Research
National Agency: CHAOS project ANR-12-BS05-0009
(http://www.chaos-project.fr), and from the UnivEarthS Labex programme
of Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). TMD
acknowledges support by the Spanish Ministerio de Economia y
competitividad (MINECO) under grant AYA2013-42627.; Based on
observations with INTEGRAL, an ESA project with instruments and science
data centre funded by ESA member states (especially the PI countries:
Denmark, France, Germany, Italy, Switzerland, Spain), and Poland, and
with the participation of Russia and the USA. Authors thank the Swift
duty scientists and science planners for supporting the XRT ToOs and of
course the PI, Neil Gehrels, for making these observations possible.
NR 68
TC 3
Z9 3
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 11
PY 2016
VL 456
IS 4
BP 3585
EP 3595
DI 10.1093/mnras/stv2901
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LM
UT WOS:000372265800013
ER
PT J
AU Earnshaw, HM
Roberts, TP
Heil, LM
Mezcua, M
Walton, DJ
Done, C
Harrison, FA
Lansbury, GB
Middleton, MJ
Sutton, AD
AF Earnshaw, Hannah M.
Roberts, Timothy P.
Heil, Lucy M.
Mezcua, Mar
Walton, Dominic J.
Done, Chris
Harrison, Fiona A.
Lansbury, George B.
Middleton, Matthew J.
Sutton, Andrew D.
TI A variable ULX and possible IMBH candidate in M51a
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: black holes; black hole physics;
galaxies: individual: M51; X-rays: binaries; X-rays: individual: M51
ULX-7
ID X-RAY SOURCES; MASS BLACK-HOLE; XMM-NEWTON OBSERVATIONS; ESO 243-49
HLX-1; SPECTRAL STATE TRANSITIONS; ACTIVE GALACTIC NUCLEI; NGC 5408 X-1;
OPTICAL COUNTERPARTS; SPIRAL-GALAXIES; ULTRALUMINOUS STATE
AB Ultraluminous X-ray source (ULX)-7, in the northern spiral arm of M51, demonstrates unusual behaviour for an ULX, with a hard X-ray spectrum but very high short-term variability. This suggests that it is not in a typical ultraluminous state. We analyse the source using archival data from XMM-Newton, Chandra and NuSTAR, and by examining optical and radio data from HST and Very Large Array. Our X-ray spectral analysis shows that the source has a hard power-law spectral shape with a photon index Gamma similar to 1.5, which persists despite the source's X-ray luminosity varying by over an order of magnitude. The power spectrum of the source features a break at 6.5(-1.1)(+0.5) x 10(-3) Hz, from a low-frequency spectral index of alpha(1) = -0.1(-0.2)(+0.5) to a high-frequency spectral index of alpha(2) = 6.5(-0.14)(+0.05), making it analogous to the low-frequency break found in the power spectra of low/hard state black holes (BHs). We can take a lower frequency limit for a corresponding high-frequency break to calculate a BH mass upper limit of 1.6 x 10(3) M-circle dot. Using the X-ray/radio Fundamental Plane, we calculate another upper limit to the BH mass of 3.5 x 10(4) M-circle dot for a BH in the low/hard state. The hard spectrum, high rms variability and mass limits are consistent with ULX-7 being an intermediate-mass BH; however we cannot exclude other interpretations of this source's interesting behaviour, most notably a neutron star with an extreme accretion rate.
C1 [Earnshaw, Hannah M.; Roberts, Timothy P.; Done, Chris; Lansbury, George B.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
[Heil, Lucy M.] Anton Pannekoek Inst, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Mezcua, Mar] Univ Montreal, Pavillon Roger Gaudry D-428, Montreal, PQ H3T 1J4, Canada.
[Mezcua, Mar] Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St, Cambridge, MA 02138 USA.
[Walton, Dominic J.; Harrison, Fiona A.] CALTECH, Pasadena, CA 91125 USA.
[Middleton, Matthew J.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Sutton, Andrew D.] NASA, George C Marshall Space Flight Ctr, Astrophys Off, ZP12, Huntsville, AL 35812 USA.
RP Earnshaw, HM (reprint author), Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
EM hannah.earnshaw@durham.ac.uk
OI Earnshaw, Hannah P/0000-0001-5857-5622
FU Science and Technology Facilities Council [ST/K501979/1, ST/L00075X/1];
NASA [G05-16099X]; ESA Member States
FX We gratefully acknowledge support from the Science and Technology
Facilities Council (HE through grant ST/K501979/1 and TR as part of
consolidated grant ST/L00075X/1) and from NASA (MM through Chandra Grant
G05-16099X). AS is supported by an appointment to the NASA Postdoctoral
Program at Marshall Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA.; The scientific
results reported in this paper are based on data obtained from the
Chandra Data Archive, and on archival observations obtained with
XMM-Newton, an ESA science mission with instruments and contributions
directly funded by ESA Member States and NASA. This research has also
made use of data obtained with NuSTAR, a project led by Caltech, funded
by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software
package, jointly developed by the ASDC (Italy) and Caltech (USA).
Further results are based on observations made with the NASA/ESA HST,
and obtained from the Hubble Legacy Archive, which is a collaboration
between the Space Telescope Science Institute (STScI/NASA), the Space
Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian
Astronomy Data Centre (CADC/NRC/CSA); and the National Radio Astronomy
Observatory, which is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
NR 85
TC 1
Z9 1
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 11
PY 2016
VL 456
IS 4
BP 3840
EP 3854
DI 10.1093/mnras/stv2945
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LM
UT WOS:000372265800032
ER
PT J
AU Siwak, M
Ogloza, W
Rucinski, SM
Moffat, AFJ
Matthews, JM
Cameron, C
Guenther, DB
Kuschnig, R
Rowe, JF
Sasselov, D
Weiss, WW
AF Siwak, Michal
Ogloza, Waldemar
Rucinski, Slavek M.
Moffat, Anthony F. J.
Matthews, Jaymie M.
Cameron, Chris
Guenther, David B.
Kuschnig, Rainer
Rowe, Jason F.
Sasselov, Dimitar
Weiss, Werner W.
TI Stable and unstable accretion in the classical T Tauri stars IM Lup and
RU Lup as observed by MOST
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: individual: RULup; stars: individual:
IMLup; stars: rotation; stars: variables: T Tauri, Herbig Ae/Be
ID MAIN-SEQUENCE STARS; QUASI-PERIODIC OSCILLATIONS; LIMB-DARKENING
COEFFICIENTS; RADIAL-VELOCITY; PHOTOMETRIC VARIABILITY; DISK ACCRETION;
LIGHT CURVES; YOUNG STARS; MAGNETOHYDRODYNAMIC SIMULATIONS; BROADENING
FUNCTIONS
AB Results of the time variability monitoring of the two classical T Tauri stars, RU Lup and IM Lup, are presented. Three photometric data sets were utilized: (1) simultaneous (same field) MOST satellite observations over four weeks in each of the years 2012 and 2013, (2) multicolour observations at the South African Astronomical Observatory in April-May of 2013, (3) archival V-filter All Sky Automated Survey (ASAS) data for nine seasons, 2001-2009. They were augmented by an analysis of high-resolution, public-domain VLT-UT2 Ultraviolet Visual Echelle Spectrograph spectra from the years 2000 to 2012. From the MOST observations, we infer that irregular light variations of RU Lup are caused by stochastic variability of hotspots induced by unstable accretion. In contrast, the MOST light curves of IM Lup are fairly regular and modulated with a period of about 7.19-7.58 d, which is in accord with ASAS observations showing a well-defined 7.247 +/- 0.026 d periodicity. We propose that this is the rotational period of IM Lup and is due to the changing visibility of two antipodal hotspots created near the stellar magnetic poles during the stable process of accretion. Re-analysis of RU Lup high-resolution spectra with the broadening function approach reveals signs of a large polar coldspot, which is fairly stable over 13 years. As the star rotates, the spot-induced depression of intensity in the broadening function profiles changes cyclically with period 3.710 58 d, which was previously found by the spectral cross-correlation method.
C1 [Siwak, Michal; Ogloza, Waldemar] Cracov Pedag Univ, Mt Suhora Astron Observ, Ul Podchorazych 2, PL-30084 Krakow, Poland.
[Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
[Moffat, Anthony F. J.] Univ Montreal, Dept Phys, CP 6128,Succursale Ctr Ville, Montreal, PQ H3C 3J7, Canada.
[Matthews, Jaymie M.; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
[Cameron, Chris] Cape Breton Univ, Dept Math Phys & Geol, 1250 Grand Lake Rd, Sydney, NS B1P 6L2, Canada.
[Guenther, David B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada.
[Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.
[Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Siwak, M (reprint author), Cracov Pedag Univ, Mt Suhora Astron Observ, Ul Podchorazych 2, PL-30084 Krakow, Poland.
EM siwak@nac.oa.uj.edu.pl
FU ESO Science Archive Facility [65.I-0404, 69.C-0481, 075.C-0292,
081.C-0779, 089.C-0299]; Polish National Science Centre
[2012/05/E/ST9/03915]; Natural Sciences and Engineering Research Council
of Canada; FRQNT (Quebec); Canadian Space Agency; Austrian Science Funds
[P22691-N16]
FX This study was based on the following:; (1) data from the MOST
satellite, a Canadian Space Agency mission jointly operated by Dynacon
Inc., the University of Toronto Institute of Aerospace Studies and the
University of British Columbia, with the assistance of the University of
Vienna,; (2) observations made at the South African Astronomical
Observatory,; (3) data obtained from the ESO Science Archive Facility
under request numbers 145841 and 145843, within the programmes ID
65.I-0404, 69.C-0481, 075.C-0292, 081.C-0779 and 089.C-0299,; (4) data
obtained from the All Sky Automated Survey (ASAS) telescope of the
Warsaw University Astronomical Observatory.; MS and WO are grateful to
the Polish National Science Centre for the grant 2012/05/E/ST9/03915.
The Natural Sciences and Engineering Research Council of Canada supports
the research of DBG, JMM, AFJM and SMR. Additional support for AFJM was
provided by FRQNT (Quebec). CC was supported by the Canadian Space
Agency. RK and WWW are supported by the Austrian Science Funds
(P22691-N16). MS and WO acknowledge Dr Hannah Worters and the entire
SAAO staff for their hospitality.
NR 84
TC 0
Z9 0
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 11
PY 2016
VL 456
IS 4
BP 3972
EP 3984
DI 10.1093/mnras/stv2848
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG7LM
UT WOS:000372265800042
ER
PT J
AU Verma, M
Friedl, MA
Finzi, AC
Phillips, N
AF Verma, Manish
Friedl, Mark A.
Finzi, Adrien C.
Phillips, Nathan
TI Multi-criteria evaluation of the suitability of growth functions for
modeling remotely sensed phenology
SO ECOLOGICAL MODELLING
LA English
DT Article
DE Phenology; Growth functions; Remote sensing; Temporal dynamics
ID NDVI TIME-SERIES; LAND-SURFACE PHENOLOGY; CLIMATE-CHANGE; FOREST CANOPY;
NORTH-AMERICA; MODIS-NDVI; SATELLITE; VEGETATION; RESOLUTION; CO2
AB Reliable information related to vegetation phenology is required to improve understanding of land-atmosphere coupling and the biosphere's response and feedbacks to climate change. The logistic function is commonly used to model bounded growth and decay and extract phenological information from remotely sensed vegetation indices. However, several other growth functions can also model bounded growth and decay and may have more desirable properties than the logistic function for capturing deciduous forest phenology. We employed three complimentary criteria and evaluated the suitability of the Gompertz, logistic, mirror-Gompertz, and Richards functions to reliably capture remotely sensed phenology of deciduous forests. Our analyses showed that although all the four growth functions fit remotely sensed data equally well, their ability to capture rapidly changing phenology early in spring and late in fall differs significantly. Using 10 years of field measurements from two deciduous forest sites in the northeastern United States, we showed that dynamics in the fraction of absorbed photosynthetically active radiation (FAPAR) phenology is asymmetric in both spring and fall. It develops more rapidly early in spring and decays more rapidly late in fall. A flexible function that can capture these asymmetric dynamics is likely to capture the phenological development and the transition dates better. Comparison with field measurements of start-of-season (SOS), end-of-season (EOS), and growing period length (GPL) confirmed this. Mean differences between modeled and observed GPL was 13.5 and 18.5 days for the Richards and logistic function, respectively, at Harvard Forest and 2.6 and 7.1 days, respectively at Hubbard Brook Forest. Our analyses also showed that FAPAR and normalized difference vegetation index have a strong linear relationship in spring, but correlate poorly in fall. Our results suggest that a flexible function line Richards is likely to be more reliable for modeling phenology and retrieving information of transitions events from remotely sensed NDVI. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Verma, Manish; Friedl, Mark A.; Phillips, Nathan] Boston Univ, Dept Earth & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA.
[Verma, Manish] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA.
[Finzi, Adrien C.] Boston Univ, Dept Biol, 5 Cummington Mall, Boston, MA USA.
RP Verma, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA.
EM Manish.K.Verma@ipl.nasa.gov
NR 50
TC 2
Z9 2
U1 8
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0304-3800
EI 1872-7026
J9 ECOL MODEL
JI Ecol. Model.
PD MAR 10
PY 2016
VL 323
BP 123
EP 132
DI 10.1016/j.ecolmodel.2015.12.005
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA DO9IP
UT WOS:000378100200012
ER
PT J
AU Aartsen, MG
Abraham, K
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Ahrens, M
Altmann, D
Anderson, T
Ansseau, I
Archinger, M
Arguelles, C
Arlen, TC
Auffenberg, J
Bai, X
Barwick, SW
Baum, V
Bay, R
Beatty, JJ
Tjus, JB
Becker, KH
Beiser, E
Benabderrahmane, ML
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Besson, DZ
Binder, G
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Borner, M
Bos, F
Bose, D
Boser, S
Botner, O
Braun, J
Brayeur, L
Bretz, HP
Buzinsky, N
Casey, J
Casier, M
Cheung, E
Chirkin, D
Christov, A
Clark, K
Classen, L
Coenders, S
Cowen, DF
Silva, AHC
Daughhetee, J
Davis, JC
Day, M
de Andre, JPAM
De Clercq, C
Rosendo, ED
Dembinski, H
De Ridder, S
Desiati, P
de Vries, KD
de Wasseige, G
de With, M
DeYoung, T
Diaz-Velez, JC
di Lorenzo, V
Dumm, JP
Dunkman, M
Eberhardt, B
Ehrhardt, T
Eichmann, B
Euler, S
Evenson, PA
Fahey, S
Fazely, AR
Feintzeig, J
Felde, J
Filimonov, K
Finley, C
Fischer-Wasels, T
Flis, S
Fosig, CC
Fuchs, T
Gaisser, TK
Gaior, R
Gallagher, J
Gerhardt, L
Ghorbani, K
Gier, D
Gladstone, L
Glagla, M
Glusenkamp, T
Goldschmidt, A
Golup, G
Gonzalez, JG
Gora, D
Grant, D
Griffith, Z
Gross, A
Ha, C
Haack, C
Ismail, AH
Hallgren, A
Halzen, F
Hansen, E
Hansmann, B
Hanson, K
Hebecker, D
Heereman, D
Helbing, K
Hellauer, R
Hickford, S
Hignight, J
Hill, GC
Hoffman, KD
Hoffmann, R
Holzapfel, K
Homeier, A
Hoshina, K
Huang, F
Huber, M
Huelsnitz, W
Hulth, PO
Hultqvist, K
In, S
Ishihara, A
Jacobi, E
Japaridze, GS
Jeong, M
Jero, K
Jurkovic, M
Kappes, A
Karg, T
Karle, A
Kauer, M
Keivani, A
Kelley, JL
Kemp, J
Kheirandish, A
Kiryluk, J
Klas, J
Klein, SR
Kohnen, G
Koirala, R
Kolanoski, H
Konietz, R
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krings, K
Kroll, G
Kroll, M
Kruckl, G
Kunnen, J
Kurahashi, N
Kuwabara, T
Labare, M
Lanfranchi, JL
Larson, MJ
Lesiak-Bzdak, M
Leuermann, M
Leuner, J
Lu, L
Lunemann, J
Madsen, J
Maggi, G
Mahn, KBM
Mandelartz, M
Maruyama, R
Mase, K
Matis, HS
Maunu, R
McNally, F
Meagher, K
Medici, M
Meli, A
Menne, T
Merino, G
Meures, T
Miarecki, S
Middell, E
Mohrmann, L
Montaruli, T
Morse, R
Nahnhauer, R
Naumann, U
Neer, G
Niederhausen, H
Nowicki, SC
Nygren, DR
Pollmann, AO
Olivas, A
Omairat, A
O'Murchadha, A
Palczewski, T
Pandya, H
Pankova, DV
Paul, L
Pepper, JA
de los Heros, CP
Pfendner, C
Pieloth, D
Pinat, E
Posselt, J
Price, PB
Przybylski, GT
Putz, J
Quinnan, M
Raab, C
Radel, L
Rameez, M
Rawlins, K
Reimann, R
Relich, M
Resconi, E
Rhode, W
Richman, M
Richter, S
Riedel, B
Robertson, S
Rongen, M
Rott, C
Ruhe, T
Ryckbosch, D
Sabbatini, L
Sander, HG
Sandrock, A
Sandroos, J
Sarkar, S
Schatto, K
Scheriau, F
Schimp, M
Schmidt, T
Schmitz, M
Schoenen, S
Schoneberg, S
Schonwald, A
Schulte, L
Schumacher, L
Seckel, D
Seunarine, S
Soldin, D
Song, M
Spiczak, GM
Spiering, C
Stahlberg, M
Stamatikos, M
Stanev, T
Stasik, A
Steuer, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strom, R
Strotjohann, NL
Sullivan, GW
Sutherland, M
Taavola, H
Taboada, I
Tatar, J
Ter-Antonyan, S
Terliuk, A
Tesic, G
Tilav, S
Toale, PA
Tobin, MN
Toscano, S
Tosi, D
Tselengidou, M
Turcati, A
Unger, E
Usner, M
Vallecorsa, S
Vandenbroucke, J
van Eijndhoven, N
Vanheule, S
van Santen, J
Veenkamp, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Wallace, A
Wallraff, M
Wandkowsky, N
Weaver, C
Wendt, C
Westerhoff, S
Whelan, BJ
Wiebe, K
Wiebusch, CH
Wille, L
Williams, DR
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, DL
Xu, XW
Xu, Y
Yanez, JP
Yodh, G
Yoshida, S
Zoll, M
AF Aartsen, M. G.
Abraham, K.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Ahrens, M.
Altmann, D.
Anderson, T.
Ansseau, I.
Archinger, M.
Arguelles, C.
Arlen, T. C.
Auffenberg, J.
Bai, X.
Barwick, S. W.
Baum, V.
Bay, R.
Beatty, J. J.
Tjus, J. Becker
Becker, K. -H.
Beiser, E.
Benabderrahmane, M. L.
Berghaus, P.
Berley, D.
Bernardini, E.
Bernhard, A.
Besson, D. Z.
Binder, G.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Boerner, M.
Bos, F.
Bose, D.
Boeser, S.
Botner, O.
Braun, J.
Brayeur, L.
Bretz, H. -P.
Buzinsky, N.
Casey, J.
Casier, M.
Cheung, E.
Chirkin, D.
Christov, A.
Clark, K.
Classen, L.
Coenders, S.
Cowen, D. F.
Silva, A. H. Cruz
Daughhetee, J.
Davis, J. C.
Day, M.
de Andre, J. P. A. M.
De Clercq, C.
Rosendo, E. del Pino
Dembinski, H.
De Ridder, S.
Desiati, P.
de Vries, K. D.
de Wasseige, G.
de With, M.
DeYoung, T.
Diaz-Velez, J. C.
di Lorenzo, V.
Dumm, J. P.
Dunkman, M.
Eberhardt, B.
Ehrhardt, T.
Eichmann, B.
Euler, S.
Evenson, P. A.
Fahey, S.
Fazely, A. R.
Feintzeig, J.
Felde, J.
Filimonov, K.
Finley, C.
Fischer-Wasels, T.
Flis, S.
Foesig, C. -C.
Fuchs, T.
Gaisser, T. K.
Gaior, R.
Gallagher, J.
Gerhardt, L.
Ghorbani, K.
Gier, D.
Gladstone, L.
Glagla, M.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Gonzalez, J. G.
Gora, D.
Grant, D.
Griffith, Z.
Gross, A.
Ha, C.
Haack, C.
Ismail, A. Haj
Hallgren, A.
Halzen, F.
Hansen, E.
Hansmann, B.
Hanson, K.
Hebecker, D.
Heereman, D.
Helbing, K.
Hellauer, R.
Hickford, S.
Hignight, J.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Holzapfel, K.
Homeier, A.
Hoshina, K.
Huang, F.
Huber, M.
Huelsnitz, W.
Hulth, P. O.
Hultqvist, K.
In, S.
Ishihara, A.
Jacobi, E.
Japaridze, G. S.
Jeong, M.
Jero, K.
Jurkovic, M.
Kappes, A.
Karg, T.
Karle, A.
Kauer, M.
Keivani, A.
Kelley, J. L.
Kemp, J.
Kheirandish, A.
Kiryluk, J.
Klaes, J.
Klein, S. R.
Kohnen, G.
Koirala, R.
Kolanoski, H.
Konietz, R.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Krings, K.
Kroll, G.
Kroll, M.
Krueckl, G.
Kunnen, J.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Lanfranchi, J. L.
Larson, M. J.
Lesiak-Bzdak, M.
Leuermann, M.
Leuner, J.
Lu, L.
Luenemann, J.
Madsen, J.
Maggi, G.
Mahn, K. B. M.
Mandelartz, M.
Maruyama, R.
Mase, K.
Matis, H. S.
Maunu, R.
McNally, F.
Meagher, K.
Medici, M.
Meli, A.
Menne, T.
Merino, G.
Meures, T.
Miarecki, S.
Middell, E.
Mohrmann, L.
Montaruli, T.
Morse, R.
Nahnhauer, R.
Naumann, U.
Neer, G.
Niederhausen, H.
Nowicki, S. C.
Nygren, D. R.
Pollmann, A. Obertacke
Olivas, A.
Omairat, A.
O'Murchadha, A.
Palczewski, T.
Pandya, H.
Pankova, D. V.
Paul, L.
Pepper, J. A.
de los Heros, C. Perez
Pfendner, C.
Pieloth, D.
Pinat, E.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Puetz, J.
Quinnan, M.
Raab, C.
Raedel, L.
Rameez, M.
Rawlins, K.
Reimann, R.
Relich, M.
Resconi, E.
Rhode, W.
Richman, M.
Richter, S.
Riedel, B.
Robertson, S.
Rongen, M.
Rott, C.
Ruhe, T.
Ryckbosch, D.
Sabbatini, L.
Sander, H. -G.
Sandrock, A.
Sandroos, J.
Sarkar, S.
Schatto, K.
Scheriau, F.
Schimp, M.
Schmidt, T.
Schmitz, M.
Schoenen, S.
Schoeneberg, S.
Schoenwald, A.
Schulte, L.
Schumacher, L.
Seckel, D.
Seunarine, S.
Soldin, D.
Song, M.
Spiczak, G. M.
Spiering, C.
Stahlberg, M.
Stamatikos, M.
Stanev, T.
Stasik, A.
Steuer, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strom, R.
Strotjohann, N. L.
Sullivan, G. W.
Sutherland, M.
Taavola, H.
Taboada, I.
Tatar, J.
Ter-Antonyan, S.
Terliuk, A.
Tesic, G.
Tilav, S.
Toale, P. A.
Tobin, M. N.
Toscano, S.
Tosi, D.
Tselengidou, M.
Turcati, A.
Unger, E.
Usner, M.
Vallecorsa, S.
Vandenbroucke, J.
van Eijndhoven, N.
Vanheule, S.
van Santen, J.
Veenkamp, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Wallace, A.
Wallraff, M.
Wandkowsky, N.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whelan, B. J.
Wiebe, K.
Wiebusch, C. H.
Wille, L.
Williams, D. R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, D. L.
Xu, X. W.
Xu, Y.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zoll, M.
TI Searches for relativistic magnetic monopoles in IceCube
SO EUROPEAN PHYSICAL JOURNAL C
LA English
DT Article
ID NEUTRINO TELESCOPE; PARTICLE; ICE; PERFORMANCE; SCATTERING; SPECTRUM;
FIELD
AB Various extensions of the Standard Model motivate the existence of stable magnetic monopoles that could have been created during an early high-energy epoch of the Universe. These primordial magnetic monopoles would be gradually accelerated by cosmic magnetic fields and could reach high velocities that make them visible in Cherenkov detectors such as IceCube. Equivalently to electrically charged particles, magnetic monopoles produce direct and indirect Cherenkov light while traversing through matter at relativistic velocities. This paper describes searches for relativistic (nu >= 0.76 c) and mildly relativistic (nu >= 0.51 c) monopoles, each using one year of data taken in 2008/2009 and 2011/2012, respectively. No monopole candidate was detected. For a velocity above 0.51 c the monopole flux is constrained down to a level of 1.55 x 10(-18) cm(-2) s(-1) sr(-1). This is an improvement of almost two orders of magnitude over previous limits.
C1 [Auffenberg, J.; Bissok, M.; Blumenthal, J.; Gier, D.; Glagla, M.; Haack, C.; Hansmann, B.; Kemp, J.; Konietz, R.; Leuermann, M.; Leuner, J.; Paul, L.; Puetz, J.; Raedel, L.; Reimann, R.; Rongen, M.; Schimp, M.; Schoenen, S.; Schumacher, L.; Stahlberg, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Phys Inst 3, D-52056 Aachen, Germany.
[Benabderrahmane, M. L.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates.
[Aartsen, M. G.; Hill, G. C.; Robertson, S.; Wallace, A.; Whelan, B. J.] Univ Adelaide, Dept Phys, Adelaide, SA 5005, Australia.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, 3211 Providence Dr, Anchorage, AK 99508 USA.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; Tatar, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Binder, G.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.; Tatar, J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[de With, M.; Hebecker, D.; Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Tjus, J. Becker; Bos, F.; Eichmann, B.; Kroll, M.; Mandelartz, M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Homeier, A.; Schulte, L.; Voge, M.] Univ Bonn, Phys Inst, Nussallee 12, D-53115 Bonn, Germany.
[Aguilar, J. A.; Ansseau, I.; Heereman, D.; Meagher, K.; Meures, T.; O'Murchadha, A.; Pinat, E.; Raab, C.] Univ Libre Bruxelles, Sci Fac CP230, B-1050 Brussels, Belgium.
[Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; de Wasseige, G.; Golup, G.; Kunnen, J.; Luenemann, J.; Maggi, G.; Toscano, S.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Gaior, R.; Ishihara, A.; Kuwabara, T.; Lu, L.; Mase, K.; Relich, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.] Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch 1, New Zealand.
[Berley, D.; Blaufuss, E.; Cheung, E.; Felde, J.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Maunu, R.; Olivas, A.; Schmidt, T.; Song, M.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
[Hansen, E.; Koskinen, D. J.; Larson, M. J.; Medici, M.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark.
[Boerner, M.; Fuchs, T.; Menne, T.; Pieloth, D.; Rhode, W.; Ruhe, T.; Sandrock, A.; Scheriau, F.; Schmitz, M.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[de Andre, J. P. A. M.; DeYoung, T.; Hignight, J.; Mahn, K. B. M.; Neer, G.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Buzinsky, N.; Grant, D.; Kopper, C.; Nowicki, S. C.; Riedel, B.; Weaver, Ch.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Altmann, D.; Classen, L.; Kappes, A.; Tselengidou, M.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[De Ridder, S.; Ismail, A. Haj; Labare, M.; Meli, A.; Ryckbosch, D.; Vanheule, S.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Ahlers, M.; Arguelles, C.; Beiser, E.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Griffith, Z.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; McNally, F.; Merino, G.; Morse, R.; Richter, S.; Sabbatini, L.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Xu, D. L.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
[Ahlers, M.; Arguelles, C.; Beiser, E.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Griffith, Z.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; McNally, F.; Merino, G.; Morse, R.; Richter, S.; Sabbatini, L.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Xu, D. L.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, 1150 Univ Ave, Madison, WI 53706 USA.
[Archinger, M.; Baum, V.; Boeser, S.; Rosendo, E. del Pino; di Lorenzo, V.; Eberhardt, B.; Ehrhardt, T.; Foesig, C. -C.; Koepke, L.; Kroll, G.; Krueckl, G.; Sander, H. -G.; Sandroos, J.; Schatto, K.; Steuer, A.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, Staudinger Weg 7, D-55099 Mainz, Germany.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Abraham, K.; Bernhard, A.; Coenders, S.; Gross, A.; Holzapfel, K.; Huber, M.; Jurkovic, M.; Krings, K.; Resconi, E.; Turcati, A.; Veenkamp, J.] Tech Univ Munich, D-85748 Garching, Germany.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Koirala, R.; Pandya, H.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Bartol Res Inst, Dept Phys & Astron, Newark, DE 19716 USA.
[Kauer, M.; Maruyama, R.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, 1 Keble Rd, Oxford OX1 3NP, England.
[Kurahashi, N.; Richman, M.] Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Ahrens, M.; Bohm, C.; Dumm, J. P.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, Dept Phys, S-10691 Stockholm, Sweden.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.; Xu, Y.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Bose, D.; In, S.; Jeong, M.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
[Clark, K.] Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada.
[Palczewski, T.; Pepper, J. A.; Toale, P. A.; Williams, D. R.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Anderson, T.; Arlen, T. C.; Cowen, D. F.; Dunkman, M.; Huang, F.; Keivani, A.; Lanfranchi, J. L.; Pankova, D. V.; Quinnan, M.; Tesic, G.] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA.
[Boersma, D. J.; Botner, O.; Euler, S.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.; Unger, E.] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden.
[Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Helbing, K.; Hickford, S.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Pollmann, A. Obertacke; Omairat, A.; Posselt, J.; Soldin, D.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Karg, T.; Kowalski, M.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stasik, A.; Stoessl, A.; Strotjohann, N. L.; Terliuk, A.; Usner, M.; van Santen, J.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Pollmann, AO; Posselt, J (reprint author), Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
EM anna.pollmann@uni-wuppertal.de; jposselt@icecube.wisc.edu
RI Tjus, Julia/G-8145-2012; Maruyama, Reina/A-1064-2013; Beatty,
James/D-9310-2011; Wiebusch, Christopher/G-6490-2012; Sarkar,
Subir/G-5978-2011; Koskinen, David/G-3236-2014;
OI Maruyama, Reina/0000-0003-2794-512X; Beatty, James/0000-0003-0481-4952;
Wiebusch, Christopher/0000-0002-6418-3008; Sarkar,
Subir/0000-0002-3542-858X; Koskinen, David/0000-0002-0514-5917; Perez de
los Heros, Carlos/0000-0002-2084-5866; Dembinski,
Hans/0000-0003-3337-3850; Arguelles Delgado, Carlos/0000-0003-4186-4182
FU U.S. National Science Foundation-Office of Polar Programs; U.S. National
Science Foundation-Physics Division; University of Wisconsin Alumni
Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid
infrastructure at the University of Wisconsin - Madison; Open Science
Grid (OSG) grid infrastructure; U.S. Department of Energy; National
Energy Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI); Natural Sciences and Engineering Research Council of
Canada; West-Grid and Compute/Calcul Canada; Swedish Research Council;
Swedish Polar Research Secretariat; Swedish National Infrastructure for
Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF); Deutsche
Forschungsgemeinschaft (DFG); Helmholtz Alliance for Astroparticle
Physics (HAP); Research Department of Plasmas with Complex Interactions
(Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus
programme; Flanders Institute to encourage scientific and technological
research in industry (IWT); Belgian Federal Science Policy Office
(Belspo); University of Oxford, United Kingdom; Marsden Fund, New
Zealand; Australian Research Council; Japan Society for Promotion of
Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland;
National Research Foundation of Korea (NRF); Danish National Research
Foundation, Denmark (DNRF)
FX We acknowledge the support from the following agencies: U.S. National
Science Foundation-Office of Polar Programs, U.S. National Science
Foundation-Physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin - Madison, the Open Science Grid (OSG)
grid infrastructure; U.S. Department of Energy, and National Energy
Research Scientific Computing Center, the Louisiana Optical Network
Initiative (LONI) grid computing resources; Natural Sciences and
Engineering Research Council of Canada, West-Grid and Compute/Calcul
Canada; Swedish Research Council, Swedish Polar Research Secretariat,
Swedish National Infrastructure for Computing (SNIC), and Knut and Alice
Wallenberg Foundation, Sweden; German Ministry for Education and
Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz
Alliance for Astroparticle Physics (HAP), Research Department of Plasmas
with Complex Interactions (Bochum), Germany; Fund for Scientific
Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to
encourage scientific and technological research in industry (IWT),
Belgian Federal Science Policy Office (Belspo); University of Oxford,
United Kingdom; Marsden Fund, New Zealand; Australian Research Council;
Japan Society for Promotion of Science (JSPS); the Swiss National
Science Foundation (SNSF), Switzerland; National Research Foundation of
Korea (NRF); Danish National Research Foundation, Denmark (DNRF).
NR 58
TC 4
Z9 4
U1 0
U2 5
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1434-6044
EI 1434-6052
J9 EUR PHYS J C
JI Eur. Phys. J. C
PD MAR 10
PY 2016
VL 76
IS 3
AR 133
DI 10.1140/epjc/s10052-016-3953-8
PG 16
WC Physics, Particles & Fields
SC Physics
GA DG7WL
UT WOS:000372294300002
ER
PT J
AU Ackermann, M
Ajello, M
Albert, A
Atwood, WB
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Bissaldi, E
Blandford, RD
Blooms, ED
Bonino, R
Bottacini, E
Bregeon, J
Bruel, P
Buehler, R
Caliandro, GA
Cameron, RA
Caragiulo, M
Caraveo, PA
Casandjian, JM
Cavazzuti, E
Cecchi, C
Charles, E
Chekhtman, A
Chiaro, G
Ciprini, S
Cohen-Tanugi, J
Conrad, J
Cutini, S
D'Ammando, F
de Angelis, A
de Palma, F
Desiante, R
Digel, SW
Di Venere, L
Drell, PS
Favuzzi, C
Fegan, SJ
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Giordano, F
Giroletti, M
Godfrey, G
Green, D
Grenier, IA
Guiriec, S
Hays, E
Hewitt, JW
Horan, D
Johannesson, G
Kuss, M
Larsson, S
Latronico, L
Li, J
Li, L
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Madejski, GM
Maldera, S
Manfreda, A
Mayer, M
Mazziotta, MN
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nuss, E
Ohsugi, T
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Pesce-Rollins, M
Petrosian, V
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Sanchez-Conde, M
Sgro, C
Siskind, EJ
Spada, F
Spandre, G
Spinelli, P
Tajima, H
Takahashi, H
Thayer, JB
Tibaldo, L
Torres, DF
Tosti, G
Troja, E
Vianello, G
Wood, KS
Zimmer, S
Rephaeli, Y
AF Ackermann, M.
Ajello, M.
Albert, A.
Atwood, W. B.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Blooms, E. D.
Bonino, R.
Bottacini, E.
Bregeon, J.
Bruel, P.
Buehler, R.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Caraveo, P. A.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiaro, G.
Ciprini, S.
Cohen-Tanugi, J.
Conrad, J.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Desiante, R.
Digel, S. W.
Di Venere, L.
Drell, P. S.
Favuzzi, C.
Fegan, S. J.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Giordano, F.
Giroletti, M.
Godfrey, G.
Green, D.
Grenier, I. A.
Guiriec, S.
Hays, E.
Hewitt, J. W.
Horan, D.
Johannesson, G.
Kuss, M.
Larsson, S.
Latronico, L.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Maldera, S.
Manfreda, A.
Mayer, M.
Mazziotta, M. N.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nuss, E.
Ohsugi, T.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Pesce-Rollins, M.
Petrosian, V.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Sanchez-Conde, M.
Sgro, C.
Siskind, E. J.
Spada, F.
Spandre, G.
Spinelli, P.
Tajima, H.
Takahashi, H.
Thayer, J. B.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Troja, E.
Vianello, G.
Wood, K. S.
Zimmer, S.
Rephaeli, Y.
CA Fermi-LAT Collaboration
TI SEARCH FOR GAMMA-RAY EMISSION FROM THE COMA CLUSTER WITH SIX YEARS OF
FERMI-LAT DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (Coma); gamma rays: galaxies: clusters
ID LARGE-AREA TELESCOPE; DIFFUSE RADIO-EMISSION; GALAXY CLUSTERS;
NONTHERMAL EMISSION; UPPER LIMITS; CONSTRAINTS; ACCELERATION; ENERGIES;
CATALOG; HALOES
AB We present results from gamma-ray observations of the Coma cluster incorporating six years of Fermi-LAT data and the newly released "Pass 8" event-level analysis. Our analysis of the region reveals low-significance residual structures within the virial radius of the cluster that are too faint for a detailed investigation with the current data. Using a likelihood approach that is free of assumptions on the spectral shape we derive upper limits on the gamma-ray flux that is expected from energetic particle interactions in the cluster. We also consider a benchmark spatial and spectral template motivated by models in which the observed radio halo is mostly emission by secondary electrons. In this case, the median expected and observed upper limits for the flux above 100MeV are 1.7 x 10(-9) ph cm(-2) s(-1) and 5.2 x 10(-9) ph cm(-2) s(-1) respectively (the latter corresponds to residual emission at the level of 1.8 sigma). These bounds are comparable to or higher than predicted levels of hadronic gamma-ray emission in cosmic-ray (CR) models with or without reacceleration of secondary electrons, although direct comparisons are sensitive to assumptions regarding the origin and propagation mode of CRs and magnetic field properties. The minimal expected.-ray flux from radio and star-forming galaxies within the Coma cluster is roughly an order of magnitude below the median sensitivity of our analysis.
C1 [Ackermann, M.; Atwood, W. B.; Buehler, R.; Mayer, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Albert, A.; Baldini, L.; Blandford, R. D.; Blooms, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Digel, S. W.; Drell, P. S.; Godfrey, G.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Tajima, H.; Thayer, J. B.; Vianello, G.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Albert, A.; Baldini, L.; Blandford, R. D.; Blooms, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Digel, S. W.; Drell, P. S.; Godfrey, G.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Tajima, H.; Thayer, J. B.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Atwood, W. B.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,CEA,IRFU,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Chiaro, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bechtol, K.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Bechtol, K.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Bellazzini, R.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bissaldi, E.; Caragiulo, M.; de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bonino, R.; Desiante, R.; Latronico, L.; Maldera, S.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bonino, R.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier, CNRS, IN2P3, Lab Universe & Particules Montpellier, F-34059 Montpellier, France.
[Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy.
[Cecchi, C.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA.
[Conrad, J.; Sanchez-Conde, M.; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.; Larsson, S.; Li, L.; Sanchez-Conde, M.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Cutini, S.] Osserv Astron Roma, INAF, I-00040 Rome, Italy.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy.
[de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Funk, S.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Green, D.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Green, D.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Green, D.; Guiriec, S.; Hays, E.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hewitt, J. W.] Univ N Florida, Dept Phys, 1 UNF Dr, Jacksonville, FL 32224 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Larsson, S.; Li, L.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Li, J.; Torres, D. F.] CSIC, Inst Space Sci IEEC, Campus UAB, E-08193 Barcelona, Spain.
[Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Mitthumsiri, W.] Mahidol Univ, Dept Phys, Fac Sci, Bangkok 10400, Thailand.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Murgia, S.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Tibaldo, L.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Rephaeli, Y.] Tel Aviv Univ, POB 39040, IL-6997801 Tel Aviv, Israel.
[Rephaeli, Y.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
RP Conrad, J (reprint author), Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.; Zimmer, S (reprint author), AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.; Reimer, O (reprint author), Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.; Rephaeli, Y (reprint author), Tel Aviv Univ, POB 39040, IL-6997801 Tel Aviv, Israel.; Rephaeli, Y (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
EM conrad@fysik.su.se; olr@slac.stanford.edu; zimmer@fysik.su.se;
yrephaeli@ucsd.edu
RI Moskalenko, Igor/A-1301-2007; Bissaldi, Elisabetta/K-7911-2016; Reimer,
Olaf/A-3117-2013; Orlando, E/R-5594-2016; Funk, Stefan/B-7629-2015;
Bonino, Raffaella/S-2367-2016; Torres, Diego/O-9422-2016; Di Venere,
Leonardo/C-7619-2017;
OI orienti, monica/0000-0003-4470-7094; Mazziotta, Mario
Nicola/0000-0001-9325-4672; Moskalenko, Igor/0000-0001-6141-458X;
Bissaldi, Elisabetta/0000-0001-9935-8106; Reimer,
Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Torres,
Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X;
Sgro', Carmelo/0000-0001-5676-6214; Zimmer, Stephan/0000-0002-5735-0082;
Pesce-Rollins, Melissa/0000-0003-1790-8018
FU National Aeronautics and Space Administration
FX This research made use of APLpy.67 We acknowledge the use of
the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration and the
use of HEALPix http://healpix.jpl.nasa.gov/ (Gorski et al. 2005).
NR 56
TC 10
Z9 10
U1 2
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 149
DI 10.3847/0004-637X/819/2/149
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700061
ER
PT J
AU Ajello, M
Baldini, L
Barbiellini, G
Bastieri, D
Bellazzini, R
Bissaldi, E
Bloom, ED
Bonino, R
Bottacini, E
Brandt, TJ
Bregeon, J
Bruel, P
Buehler, R
Caliandro, GA
Cameron, RA
Caragiulo, M
Cavazzuti, E
Charles, E
Chekhtman, A
Ciprini, S
Cohen-Tanugi, J
Condon, B
Costanza, F
Cutini, S
D'Ammando, F
de Palma, F
Desiante, R
Di Lalla, N
Di Mauro, M
Di Venere, L
Drell, PS
Dubner, G
Dumora, D
Duvidovich, L
Favuzzi, C
Focke, WB
Fusco, P
Gargano, F
Gasparrini, D
Giacani, E
Giglietto, N
Glanzman, T
Green, DA
Grenier, IA
Guiriec, S
Hays, E
Hewitt, JW
Hill, AB
Horan, D
Jogler, T
Johannesson, G
Jung-Richardt, I
Kensei, S
Kuss, M
Larsson, S
Latronico, L
Lemoine-Goumard, M
Li, J
Li, L
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Magill, J
Maldera, S
Manfreda, A
Mayer, M
Mazziotta, MN
McEnery, JE
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monzani, ME
Morselli, A
Moskalenko, IV
Negro, M
Nuss, E
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Reposeur, T
Schmid, J
Schulz, A
Sgro, C
Simone, D
Siskind, EJ
Spada, F
Spandre, G
Spinelli, P
Thayer, JB
Tibaldo, L
Torres, DF
Tosti, G
Troja, E
Uchiyama, Y
Vianello, G
Vink, J
Wood, KS
Yassine, M
AF Ajello, M.
Baldini, L.
Barbiellini, G.
Bastieri, D.
Bellazzini, R.
Bissaldi, E.
Bloom, E. D.
Bonino, R.
Bottacini, E.
Brandt, T. J.
Bregeon, J.
Bruel, P.
Buehler, R.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Cavazzuti, E.
Charles, E.
Chekhtman, A.
Ciprini, S.
Cohen-Tanugi, J.
Condon, B.
Costanza, F.
Cutini, S.
D'Ammando, F.
de Palma, F.
Desiante, R.
Di Lalla, N.
Di Mauro, M.
Di Venere, L.
Drell, P. S.
Dubner, G.
Dumora, D.
Duvidovich, L.
Favuzzi, C.
Focke, W. B.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giacani, E.
Giglietto, N.
Glanzman, T.
Green, D. A.
Grenier, I. A.
Guiriec, S.
Hays, E.
Hewitt, J. W.
Hill, A. B.
Horan, D.
Jogler, T.
Johannesson, G.
Jung-Richardt, I.
Kensei, S.
Kuss, M.
Larsson, S.
Latronico, L.
Lemoine-Goumard, M.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Magill, J.
Maldera, S.
Manfreda, A.
Mayer, M.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Negro, M.
Nuss, E.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Reposeur, T.
Schmid, J.
Schulz, A.
Sgro, C.
Simone, D.
Siskind, E. J.
Spada, F.
Spandre, G.
Spinelli, P.
Thayer, J. B.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Troja, E.
Uchiyama, Y.
Vianello, G.
Vink, J.
Wood, K. S.
Yassine, M.
TI DEEP MORPHOLOGICAL AND SPECTRAL STUDY OF THE SNR RCW 86 WITH FERMI-LAT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; cosmic rays; ISM: individual objects (RCW 86)
ID LARGE-AREA TELESCOPE; RAY SYNCHROTRON EMISSION; SUPERNOVA REMNANT;
X-RAY; COSMIC-RAYS; PARTICLE-ACCELERATION; SUZAKU OBSERVATION; GALACTIC
PLANE; SOURCE CATALOG; SHOCK FRONTS
AB RCW 86 is a young supernova remnant (SNR) showing a shell-type structure at several wavelengths and is thought to be an efficient cosmic-ray (CR) accelerator. Earlier Fermi Large Area Telescope results reported the detection of.-ray emission coincident with the position of RCW 86 but its origin (leptonic or hadronic) remained unclear due to the poor statistics. Thanks to 6.5 years of data acquired by the Fermi-LAT and the new event reconstruction Pass 8, we report the significant detection of spatially extended emission coming from RCW 86. The spectrum is described by a power-law function with a very hard photon index (Gamma= 1.42 +/- 0.1(stat) +/- 0.06(syst)) in the 0.1-500 GeV range and an energy flux above 100 MeV of (2.91. 0.8(stat). 0.12(syst)) 10-11 erg cm(-2) s(-1). Gathering all the available multiwavelength (MWL) data, we perform a broadband modeling of the nonthermal emission of RCW 86 to constrain parameters of the nearby medium and bring new hints about the origin of the gamma-ray emission. For the whole SNR, the modeling favors a leptonic scenario in the framework of a two-zone model with an average magnetic field of 10.2 +/- 0.7 mu G and a limit on the maximum energy injected into protons of 2. x. 10(49) erg for a density of 1 cm(-3). In addition, parameter values are derived for the north-east and south-west (SW) regions of RCW 86, providing the first indication of a higher magnetic field in the SW region.
C1 [Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Baldini, L.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Di Mauro, M.; Drell, P. S.; Focke, W. B.; Glanzman, T.; Hill, A. B.; Jogler, T.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. B.; Vianello, G.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Baldini, L.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Di Mauro, M.; Drell, P. S.; Focke, W. B.; Glanzman, T.; Hill, A. B.; Jogler, T.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Orlando, E.; Paneque, D.; Pesce-Rollins, M.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. B.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bellazzini, R.; Di Lalla, N.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bissaldi, E.; Caragiulo, M.; Costanza, F.; de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Simone, D.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bonino, R.; Desiante, R.; Latronico, L.; Maldera, S.; Negro, M.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bonino, R.; Negro, M.] Univ Torino, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[Brandt, T. J.; Guiriec, S.; Hays, E.; McEnery, J. E.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Yassine, M.] Univ Montpellier, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34059 Montpellier, France.
[Bruel, P.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Caliandro, G. A.] Consorzio Interuniv Fis Spaziale CIFS, I-10133 Turin, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00133 Rome, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA.
[Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Condon, B.; Dumora, D.; Lemoine-Goumard, M.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, BP120, F-33175 Gradignan, France.
[Cutini, S.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[D'Ammando, F.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Dubner, G.; Duvidovich, L.; Giacani, E.] Inst Astron & Fis Espacio, Parbellon IAFE, Cdad Univ, RA-1428 Buenos Aires, DF, Argentina.
[Green, D. A.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
[Grenier, I. A.; Schmid, J.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France.
[Hewitt, J. W.] Univ N Florida, Dept Phys, 1 UNF Dr, Jacksonville, FL 32224 USA.
[Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Jung-Richardt, I.] Univ Erlangen Nurnberg, Schlosspl 4, D-91054 Erlangen, Germany.
[Kensei, S.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Larsson, S.; Li, L.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Larsson, S.; Li, L.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Li, J.; Torres, D. F.] Inst Space Sci IEEC CSIC, Campus UAB, E-08193 Barcelona, Spain.
[Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Magill, J.; McEnery, J. E.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Magill, J.; McEnery, J. E.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mitthumsiri, W.] Mahidol Univ, Dept Phys, Fac Sci, Bangkok 10400, Thailand.
[Mizuno, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Tibaldo, L.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Uchiyama, Y.] Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan.
[Vink, J.] Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
RP Caragiulo, M (reprint author), Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.; Caragiulo, M (reprint author), Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.; Caragiulo, M (reprint author), Politecn Bari, I-70126 Bari, Italy.; Condon, B; Lemoine-Goumard, M (reprint author), Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, BP120, F-33175 Gradignan, France.
EM micaela.caragiulo@ba.infn.it; condon@cenbg.in2p3.fr;
lemoine@cenbg.in2p3.fr
RI Moskalenko, Igor/A-1301-2007; Green, David/E-9609-2010; Reimer,
Olaf/A-3117-2013; Orlando, E/R-5594-2016; Bonino, Raffaella/S-2367-2016;
Torres, Diego/O-9422-2016; Di Venere, Leonardo/C-7619-2017; Bissaldi,
Elisabetta/K-7911-2016;
OI DI MAURO, MATTIA/0000-0003-2759-5625; Mazziotta, Mario
Nicola/0000-0001-9325-4672; Moskalenko, Igor/0000-0001-6141-458X; Green,
David/0000-0003-3189-9998; Reimer, Olaf/0000-0001-6953-1385; Torres,
Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X;
Gargano, Fabio/0000-0002-5055-6395; Sgro', Carmelo/0000-0001-5676-6214;
Pesce-Rollins, Melissa/0000-0003-1790-8018; Hill,
Adam/0000-0003-3470-4834; Bissaldi, Elisabetta/0000-0001-9935-8106;
orienti, monica/0000-0003-4470-7094
FU CONICET; ANPCyT (Argentina)
FX The Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the KA. Wallenberg Foundation, the Swedish
Research Council and the Swedish National Space Board in Sweden.
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France. GD and EG
are members of CIC-CONICET (Argentina), LD is Fellow of CONICET
(Argentina). They are supported through grants from CONICET and ANPCyT
(Argentina). We acknowledge to Estela Reynoso and Anne Green who
collaborated in the first stages of the HI data acquisition and
preocessing.
NR 55
TC 1
Z9 1
U1 2
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 98
DI 10.3847/0004-637X/819/2/98
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700010
ER
PT J
AU Assef, RJ
Walton, DJ
Brightman, M
Stern, D
Alexander, D
Bauer, F
Blain, AW
Diaz-Santos, T
Eisenhardt, PRM
Finkelstein, SL
Hickox, RC
Tsai, CW
Wu, JW
AF Assef, R. J.
Walton, D. J.
Brightman, M.
Stern, D.
Alexander, D.
Bauer, F.
Blain, A. W.
Diaz-Santos, T.
Eisenhardt, P. R. M.
Finkelstein, S. L.
Hickox, R. C.
Tsai, C-W
Wu, J. W.
TI HOT DUST OBSCURED GALAXIES WITH EXCESS BLUE LIGHT: DUAL AGN OR SINGLE
AGN UNDER EXTREME CONDITIONS?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: evolution; galaxies: high-redshift;
infrared: galaxies; quasars: general
ID ACTIVE GALACTIC NUCLEI; HARD X-RAY; STAR-FORMING GALAXIES; DIGITAL SKY
SURVEY; ULTRALUMINOUS INFRARED GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS;
REDSHIFT RADIO GALAXIES; XMM-NEWTON OBSERVATIONS; SIMILAR-TO 2;
BROAD-BAND
AB Hot dust-obscured galaxies (Hot DOGs) are a population of hyper-luminous infrared galaxies identified by the Wide-field Infrared Survey Explorer (WISE) mission from their very red mid-IR colors, and characterized by hot dust temperatures (T > 60 K). Several studies have shown clear evidence that the IR emission in these objects is powered by a highly dust-obscured active galactic nucleus (AGN) that shows close to Compton-thick absorption at X-ray wavelengths. Thanks to the high AGN obscuration, the host galaxy is easily observable, and has UV/optical colors usually consistent with those of a normal galaxy. Here we discuss a sub-population of eight Hot DOGs that show enhanced rest-frame UV/optical emission. We discuss three scenarios that might explain the excess UV emission: (i) unobscured light leaked from the AGN by reflection over the dust or by partial coverage of the accretion disk; (ii) a second unobscured AGN in the system; or (iii) a luminous young starburst. X-ray observations can help discriminate between these scenarios. We study in detail the blue excess Hot DOG WISE J020446.13-050640.8, which was serendipitously observed by Chandra/ACIS-I for 174.5 ks. The X-ray spectrum is consistent with a single, hyper-luminous, highly absorbed AGN, and is strongly inconsistent with the presence of a secondary unobscured AGN. Based on this, we argue that the excess blue emission in this object is most likely either due to reflection or a co-eval starburst. We favor the reflection scenario as the unobscured star formation rate needed to power the UV/optical emission would be greater than or similar to 1000M(circle dot) yr(-1). Deep polarimetry observations could confirm the reflection hypothesis.
C1 [Assef, R. J.; Diaz-Santos, T.] Univ Diego Portales, Nucleo Astron, Fac Ingn, Ave Ejercito Libertador 441, Santiago, Chile.
[Walton, D. J.; Brightman, M.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Stern, D.; Eisenhardt, P. R. M.; Tsai, C-W] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-236, Pasadena, CA 91109 USA.
[Alexander, D.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Bauer, F.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Casilla 306, Santiago 22, Chile.
[Bauer, F.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
[Bauer, F.] MAS, Millennium Inst Astrophys, Nuncio Monsenor Sotero Sanz 100, Providencia, Santiago De Chi, Chile.
[Blain, A. W.] Univ Leicester, Phys & Astron, 1 Univ Rd, Leicester LE1 7RH, Leics, England.
[Finkelstein, S. L.] Univ Texas Austin, 2515 Speedway,Stop C1400, Austin, TX 78712 USA.
[Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA.
[Wu, J. W.] UCLA Astron, POB 951547, Los Angeles, CA 90095 USA.
RP Assef, RJ (reprint author), Univ Diego Portales, Nucleo Astron, Fac Ingn, Ave Ejercito Libertador 441, Santiago, Chile.
EM roberto.assef@mail.udp.cl
FU Gemini-CONICYT [32120009]; FONDECYT [1151408, 1151239]; CONICYT-Chile
[Basal-CATA PFB-06/2007, FONDECYT 1141218, "EMBIGGEN" Anillo ACT1101];
Ministry of Economy, Development, and Tourism's Millennium Science
Initiative [IC120009]; ALMA-CONYCIT [31130005]; National Aeronautics and
Space Administration [13-ADAP13-0092]; National Aeronautics and Space
Administration; Alfred P. Sloan Foundation; National Science Foundation;
U.S. Department of Energy Office of Science; University of Arizona;
Brazilian Participation Group; Brookhaven National Laboratory; Carnegie
Mellon University; University of Florida; French Participation Group;
German Participation Group; Harvard University; Instituto de Astrofisica
de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns
Hopkins University; Lawrence Berkeley National Laboratory; Max Planck
Institute for Astrophysics; Max Planck Institute for Extraterrestrial
Physics; New Mexico State University; New York University; Ohio State
University; Pennsylvania State University; University of Portsmouth;
Princeton University; Spanish Participation Group; University of Tokyo;
University of Utah; Vanderbilt University; University of Virginia;
University of Washington; Yale University
FX We thank Sangeeta Malhotra and James Rhoads for providing us with
optical imaging data for the Cetus field. We also thank the anonymous
referee for useful comments and suggestions. R.J.A. was supported by
Gemini-CONICYT grant number 32120009 and FONDECYT grant number 1151408.
FEB acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007,
FONDECYT 1141218, "EMBIGGEN" Anillo ACT1101), and the Ministry of
Economy, Development, and Tourism's Millennium Science Initiative
through grant IC120009, awarded to The Millennium Institute of
Astrophysics, MAS. T.D.-S. acknowledges support from ALMA-CONYCIT
project 31130005 and FONDECYT 1151239. This material is based upon work
supported by the National Aeronautics and Space Administration under
Proposal No. 13-ADAP13-0092 issued through the Astrophysics Data
Analysis Program. The scientific results reported in this article are
based to a significant degree on data obtained from the Chandra Data
Archive. This publication makes use of data products from the Wide-field
Infrared Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration. This work is based in part on observations made with the
Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. The WIYN Observatory is a joint facility of the University of
Wisconsin-Madison, Indiana University, Yale University, and the National
Optical Astronomy Observatory. Funding for SDSS-III has been provided by
the Alfred P. Sloan Foundation, the Participating Institutions, the
National Science Foundation, and the U.S. Department of Energy Office of
Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is
managed by the Astrophysical Research Consortium for the Participating
Institutions of the SDSS-III Collaboration including the University of
Arizona, the Brazilian Participation Group, Brookhaven National
Laboratory, Carnegie Mellon University, University of Florida, the
French Participation Group, the German Participation Group, Harvard
University, the Instituto de Astrofisica de Canarias, the Michigan
State/Notre Dame/JINA Participation Group, Johns Hopkins University,
Lawrence Berkeley National Laboratory, Max Planck Institute for
Astrophysics, Max Planck Institute for Extraterrestrial Physics, New
Mexico State University, New York University, Ohio State University,
Pennsylvania State University, University of Portsmouth, Princeton
University, the Spanish Participation Group, University of Tokyo,
University of Utah, Vanderbilt University,University of Virginia,
University of Washington, and Yale University. Some of the observations
reported here were obtained at the MMT Observatory, a joint facility of
the Smithsonian Institution and the University of Arizona.
NR 98
TC 5
Z9 5
U1 2
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 111
DI 10.3847/0004-637X/819/2/111
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700023
ER
PT J
AU Balokovic, M
Paneque, D
Madejski, G
Furniss, A
Chiang, J
Ajell, M
Alexander, DM
Barret, D
Blandford, RD
Boggs, SE
Christensen, FE
Craig, WW
Forster, K
Giommi, P
Grefenstette, B
Hailey, C
Harrison, FA
Hornstrup, A
Kitaguchi, T
Koglin, JE
Madsen, KK
Mao, PH
Miyasaka, H
Mori, K
Perri, M
Pivovaroff, MJ
Puccetti, S
Rana, V
Stern, D
Tagliaferri, G
Urry, CM
Estergaard, NJW
Zhang, WW
Zoglauer, A
Archambault, S
Archer, A
Barnacka, A
Benbow, W
Bird, R
Buckley, JH
Bugaev, V
Cerruti, M
Chen, X
Ciupik, L
Connolly, MP
Cui, W
Dickinson, HJ
Dumm, J
Eisch, JD
Falcone, A
Feng, Q
Finley, JP
Fleischhack, H
Fortson, L
Griffin, S
Griffiths, ST
Grube, J
Gyuk, G
Huetten, M
Hakansson, N
Holder, J
Humensky, TB
Johnson, CA
Kaaret, P
Kertzman, M
Khassen, Y
Kieda, D
Krause, M
Krennrich, F
Lang, MJ
Maier, G
McArthur, S
Meagher, K
Moriarty, P
Nelson, T
Nieto, D
Ong, RA
Park, N
Poiil, M
Popkow, A
Pueschel, E
Reynolds, PT
Richards, GT
Roache, E
Santander, M
Sembroski, GH
Shahinyan, K
Smith, AW
Staszak, D
Telezhinsky, I
Todd, NW
Tucci, JV
Tyler, J
Vincent, S
Weinstein, A
Wilhelm, A
Williams, DA
Zitzer, B
Ahnen, ML
Ansoldi, S
Antonelli, LA
Antoranz, P
Babic, A
Banerjee, B
Bangale, P
de Almeida, UB
Barrio, JA
Gonzalez, JB
Bednarek, W
Bernardini, E
Biasuzzi, B
Biland, A
Blanch, O
Bonnefoy, S
Bonnoli, G
Borracci, F
Bretz, T
Carmona, E
Carosi, A
Chatterjee, A
Clavero, R
Colin, P
Colombo, E
Contreras, JL
Cortina, J
Covino, S
Da Vela, P
Dazzi, F
De Angelis, A
De Lotto, B
Wilhelmi, ED
Mendez, CD
Di Pierro, E
Prester, DD
Dorner, D
Doro, M
Einecke, S
Elsaesser, D
Fernandez-Barral, A
Fidalgo, D
Fonseca, MV
Font, L
Frantzen, K
Fruck, C
Galindo, D
Lopez, JG
Garczarczyk, M
Terrats, DG
Gaug, M
Giammaria, P
Glawion, D
Gouinovic, N
Munoz, AG
Guberman, D
Hahn, A
Hanabata, Y
Hayashida, M
Herrera, J
Hose, J
Hrupec, D
Hughes, G
Idec, W
Kodani, K
Konno, Y
Kubo, H
Kushida, J
La Barbera, A
Lelas, D
Lindfors, E
Lombardi, S
Longo, F
Lopez, M
Lopez-Coto, R
Lopez-Oramas, A
Lorenz, E
Majumdar, P
Makariev, M
Mallot, K
Maneva, G
Manganaro, M
Mannheim, K
Maraschi, L
Marcote, B
Mariotti, M
Martinez, M
Mazin, D
Menzel, U
Miranda, JM
Mirzoyan, R
Moralejo, A
Moretti, E
Nakajima, D
Neustroev, V
Niedzwiecki, A
Rosillo, MN
Nilsson, K
Nishijima, K
Noda, K
Orito, R
Overkemping, A
Paiano, S
Palacio, J
Palatiello, M
Paoletti, R
Paredes, JM
Paredes-Fortuny, X
Persic, M
Poutanen, J
Moroni, PGP
Prandini, E
Puljak, I
Rhode, W
Ribo, M
Rico, J
Garcia, JR
Saito, T
Satalecka, K
Scapin, V
Schultz, C
Schweizer, T
Shore, SN
Sillanpaa, A
Sitarek, J
Snidaric, I
Sobczynska, D
Stamerra, A
Steinbring, T
Strzys, M
Takalo, L
Takami, H
Tavecchio, F
Temnikov, P
Terzic, T
Tescaro, D
Teshima, M
Thaele, J
Torres, DF
Toyama, T
Treves, A
Verguilov, V
Vovk, I
Ward, JE
Will, M
Wu, MH
Zanin, R
Perkins, J
Verrecchia, F
Leto, C
Bottcher, M
Villata, M
Raiteri, CM
Acosta-Pulido, JA
Bachev, R
Berdyugin, A
Blinov, DA
Carnerero, MI
Chen, WP
Chinchilla, P
Damljanovic, G
Eswaraiah, C
Grisinna, TS
Ibryamov, S
Jordan, B
Jorstad, SG
Joshi, M
Kopatskaya, EN
Kurtanidze, OM
Kurtanidze, SO
Larionova, EG
Larionova, LV
Larionov, VM
Latev, G
Lin, HC
Marscher, AP
Mokrushina, AA
Morozova, DA
Nikolashvili, MG
Semkov, E
Smith, PS
Strigachev, A
Troitskaya, YV
Troitsky, IS
Vince, O
Barnes, J
Guver, T
Moody, JW
Sadun, AC
Sun, S
Hovatta, T
Richards, JL
Max-Moerbeck, W
Readhead, ACR
Lahteenmaki, A
Tornikoski, M
Tammi, J
Ramakrishnan, V
Reinthal, R
Angelakis, E
Fuhrmann, L
Myserlis, I
Karamanavis, V
Sievers, A
Ungerechts, H
Zensus, JA
AF Balokovic, M.
Paneque, D.
Madejski, G.
Furniss, A.
Chiang, J.
Ajell, M.
Alexander, D. M.
Barret, D.
Blandford, R. D.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Forster, K.
Giommi, P.
Grefenstette, B.
Hailey, C.
Harrison, F. A.
Hornstrup, A.
Kitaguchi, T.
Koglin, J. E.
Madsen, K. K.
Mao, P. H.
Miyasaka, H.
Mori, K.
Perri, M.
Pivovaroff, M. J.
Puccetti, S.
Rana, V.
Stern, D.
Tagliaferri, G.
Urry, C. M.
Estergaard, N. J. W.
Zhang, W. W.
Zoglauer, A.
Archambault, S.
Archer, A.
Barnacka, A.
Benbow, W.
Bird, R.
Buckley, J. H.
Bugaev, V.
Cerruti, M.
Chen, X.
Ciupik, L.
Connolly, M. P.
Cui, W.
Dickinson, H. J.
Dumm, J.
Eisch, J. D.
Falcone, A.
Feng, Q.
Finley, J. P.
Fleischhack, H.
Fortson, L.
Griffin, S.
Griffiths, S. T.
Grube, J.
Gyuk, G.
Huetten, M.
Hakansson, N.
Holder, J.
Humensky, T. B.
Johnson, C. A.
Kaaret, P.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krause, M.
Krennrich, F.
Lang, M. J.
Maier, G.
McArthur, S.
Meagher, K.
Moriarty, P.
Nelson, T.
Nieto, D.
Ong, R. A.
Park, N.
Poiil, M.
Popkow, A.
Pueschel, E.
Reynolds, P. T.
Richards, G. T.
Roache, E.
Santander, M.
Sembroski, G. H.
Shahinyan, K.
Smith, A. W.
Staszak, D.
Telezhinsky, I.
Todd, N. W.
Tucci, J. V.
Tyler, J.
Vincent, S.
Weinstein, A.
Wilhelm, A.
Williams, D. A.
Zitzer, B.
Ahnen, M. L.
Ansoldi, S.
Antonelli, L. A.
Antoranz, P.
Babic, A.
Banerjee, B.
Bangale, P.
Barres de Almeida, U.
Barrio, J. A.
Becerra Gonzalez, J.
Bednarek, W.
Bernardini, E.
Biasuzzi, B.
Biland, A.
Blanch, O.
Bonnefoy, S.
Bonnoli, G.
Borracci, F.
Bretz, T.
Carmona, E.
Carosi, A.
Chatterjee, A.
Clavero, R.
Colin, P.
Colombo, E.
Contreras, J. L.
Cortina, J.
Covino, S.
Da Vela, P.
Dazzi, F.
De Angelis, A.
De Lotto, B.
de Ona Wilhelmi, E.
Delgado Mendez, C.
Di Pierro, E.
Prester, D. Dominis
Dorner, D.
Doro, M.
Einecke, S.
Elsaesser, D.
Fernandez-Barral, A.
Fidalgo, D.
Fonseca, M. V.
Font, L.
Frantzen, K.
Fruck, C.
Galindo, D.
Garcia Lopez, J.
Garczarczyk, M.
Terrats, D. Garrido
Gaug, M.
Giammaria, P.
Glawion (Eisenacher), D.
Gouinovic, N.
Gonzalez Munoz, A.
Guberman, D.
Hahn, A.
Hanabata, Y.
Hayashida, M.
Herrera, J.
Hose, J.
Hrupec, D.
Hughes, G.
Idec, W.
Kodani, K.
Konno, Y.
Kubo, H.
Kushida, J.
La Barbera, A.
Lelas, D.
Lindfors, E.
Lombardi, S.
Longo, F.
Lopez, M.
Lopez-Coto, R.
Lopez-Oramas, A.
Lorenz, E.
Majumdar, P.
Makariev, M.
Mallot, K.
Maneva, G.
Manganaro, M.
Mannheim, K.
Maraschi, L.
Marcote, B.
Mariotti, M.
Martinez, M.
Mazin, D.
Menzel, U.
Miranda, J. M.
Mirzoyan, R.
Moralejo, A.
Moretti, E.
Nakajima, D.
Neustroev, V.
Niedzwiecki, A.
Rosillo, M. Nievas
Nilsson, K.
Nishijima, K.
Noda, K.
Orito, R.
Overkemping, A.
Paiano, S.
Palacio, J.
Palatiello, M.
Paoletti, R.
Paredes, J. M.
Paredes-Fortuny, X.
Persic, M.
Poutanen, J.
Moroni, P. G. Prada
Prandini, E.
Puljak, I.
Rhode, W.
Ribo, M.
Rico, J.
Rodriguez Garcia, J.
Saito, T.
Satalecka, K.
Scapin, V.
Schultz, C.
Schweizer, T.
Shore, S. N.
Sillanpaa, A.
Sitarek, J.
Snidaric, I.
Sobczynska, D.
Stamerra, A.
Steinbring, T.
Strzys, M.
Takalo, L.
Takami, H.
Tavecchio, F.
Temnikov, P.
Terzic, T.
Tescaro, D.
Teshima, M.
Thaele, J.
Torres, D. F.
Toyama, T.
Treves, A.
Verguilov, V.
Vovk, I.
Ward, J. E.
Will, M.
Wu, M. H.
Zanin, R.
Perkins, J.
Verrecchia, F.
Leto, C.
Boettcher, M.
Villata, M.
Raiteri, C. M.
Acosta-Pulido, J. A.
Bachev, R.
Berdyugin, A.
Blinov, D. A.
Carnerero, M. I.
Chen, W. P.
Chinchilla, P.
Damljanovic, G.
Eswaraiah, C.
Grisinna, T. S.
Ibryamov, S.
Jordan, B.
Jorstad, S. G.
Joshi, M.
Kopatskaya, E. N.
Kurtanidze, O. M.
Kurtanidze, S. O.
Larionova, E. G.
Larionova, L. V.
Larionov, V. M.
Latev, G.
Lin, H. C.
Marscher, A. P.
Mokrushina, A. A.
Morozova, D. A.
Nikolashvili, M. G.
Semkov, E.
Smith, P. S.
Strigachev, A.
Troitskaya, Yu. V.
Troitsky, I. S.
Vince, O.
Barnes, J.
Guever, T.
Moody, J. W.
Sadun, A. C.
Sun, S.
Hovatta, T.
Richards, J. L.
Max-Moerbeck, W.
Readhead, A. C. R.
Lahteenmaki, A.
Tornikoski, M.
Tammi, J.
Ramakrishnan, V.
Reinthal, R.
Angelakis, E.
Fuhrmann, L.
Myserlis, I.
Karamanavis, V.
Sievers, A.
Ungerechts, H.
Zensus, J. A.
CA NuSTAR Team
VERITAS Collaboration
MAGIC Collaboration
TI MULTIWAVELENGTH STUDY OF QUIESCENT STATES OF Mrk 421 WITH UNPRECEDENTED
HARD X-RAY COVERAGE PROVIDED BY NuSTAR IN 2013
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (Markarian 421); galaxies: active; gamma
rays: general; radiation mechanisms: nonthermal; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS;
PARTICLE-ACCELERATION; LAC OBJECTS; CORRELATED VARIABILITY; TEV BLAZARS;
ELECTRON ACCELERATION; MAGNETIC RECONNECTION; BACKGROUND-RADIATION
AB We present coordinated multiwavelength observations of the bright, nearby BL Lacertae object Mrk 421 taken in 2013 January-March, involving GASP-WEBT, Swift, NuSTAR, Fermi-LAT, MAGIC, VERITAS, and other collaborations and instruments, providing data from radio to very high energy. (VHE).-ray bands. NuSTAR yielded previously unattainable sensitivity in the 3-79. keV range, revealing that the spectrum softens when the source is dimmer until the X-ray spectral shape saturates into a steep Gamma approximate to 3 power law, with no evidence for an exponential cutoff or additional hard components up to similar to 80. keV. For the first time, we observed both the synchrotron and the inverse-Compton peaks of the spectral energy distribution (SED) simultaneously shifted to frequencies below the typical quiescent state by an order of magnitude. The fractional variability as a function of photon energy shows a double-bump structure that relates to the two bumps of the broadband SED. In each bump, the variability increases with energy, which, in the framework of the synchrotron self-Compton model, implies that the electrons with higher energies are more variable. The measured multi band variability, the significant X-ray-to-VHE correlation down to some of the lowest fluxes ever observed in both bands, the lack of correlation between optical/UV and X-ray flux, the low degree of polarization and its significant (random) variations, the short estimated electron cooling time, and the significantly longer variability timescale observed in the NuSTAR light curves point toward in situ electron acceleration and suggest that there are multiple compact regions contributing to the broadband emission of Mrk 421 during low-activity states.
C1 [Balokovic, M.; Forster, K.; Grefenstette, B.; Harrison, F. A.; Madsen, K. K.; Mao, P. H.; Miyasaka, H.; Rana, V.; Hovatta, T.; Readhead, A. C. R.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Paneque, D.; Bangale, P.; Barres de Almeida, U.; Borracci, F.; Colin, P.; Dazzi, F.; Doro, M.; Fruck, C.; Hahn, A.; Hose, J.; Lorenz, E.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Moretti, E.; Noda, K.; Rodriguez Garcia, J.; Schweizer, T.; Strzys, M.; Teshima, M.; Toyama, T.; Vovk, I.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Madejski, G.; Chiang, J.; Blandford, R. D.; Koglin, J. E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA.
[Madejski, G.; Chiang, J.; Blandford, R. D.; Koglin, J. E.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Furniss, A.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Ajell, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Barret, D.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Barret, D.] CNRS, Inst Rech Astrophys & Planetol, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France.
[Boggs, S. E.; Craig, W. W.; Pivovaroff, M. J.; Zoglauer, A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.; Hornstrup, A.; Estergaard, N. J. W.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Giommi, P.; Perri, M.; Puccetti, S.; Verrecchia, F.; Leto, C.] ASI Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy.
[Hailey, C.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Kitaguchi, T.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Kitaguchi, T.] Hiroshima Univ, Core Res Energet Universe, Higashihiroshima, Hiroshima 7398526, Japan.
[Mori, K.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Perri, M.; Puccetti, S.; Verrecchia, F.; Leto, C.] Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tagliaferri, G.] Osservatorio Astronomico Brera, INAF, Via E Bianchi 46, I-23807 Merate, Italy.
[Urry, C. M.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, POB 208120, New Haven, CT 06520 USA.
[Zhang, W. W.; Smith, A. W.; Becerra Gonzalez, J.; Perkins, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Archambault, S.; Griffin, S.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Archer, A.; Buckley, J. H.; Bugaev, V.; Todd, N. W.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Barnacka, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Benbow, W.; Cerruti, M.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Bird, R.; Khassen, Y.; Pueschel, E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Chen, X.; Hakansson, N.; Poiil, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Chen, X.; Fleischhack, H.; Huetten, M.; Krause, M.; Maier, G.; Poiil, M.; Telezhinsky, I.; Vincent, S.; Wilhelm, A.; Bernardini, E.; Garczarczyk, M.; Mallot, K.] Deutsch Elektronen Synchrotron DESY, Platanenallee 6, D-15738 Zeuthen, Germany.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Connolly, M. P.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland.
[Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Richards, J. L.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
[Dickinson, H. J.; Eisch, J. D.; Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Dumm, J.; Fortson, L.; Nelson, T.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA.
[Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Humensky, T. B.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Humensky, T. B.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[McArthur, S.; Park, N.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Meagher, K.; Richards, G. T.] Georgia Inst Technol, Sch Phys, 837 State St NW, Atlanta, GA 30332 USA.
[Meagher, K.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA.
[Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Sci, Cork, Ireland.
[Santander, M.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Smith, A. W.; Becerra Gonzalez, J.] Univ Maryland, College Pk, MD 20742 USA.
[Zitzer, B.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Ahnen, M. L.; Biland, A.; Hughes, G.; Prandini, E.] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
[Ansoldi, S.; Biasuzzi, B.; De Lotto, B.; Longo, F.; Palatiello, M.; Persic, M.] Univ Udine, I-33100 Udine, Italy.
[Ansoldi, S.; Biasuzzi, B.; De Lotto, B.; Longo, F.; Palatiello, M.; Persic, M.] INFN Trieste, I-33100 Udine, Italy.
[Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; Di Pierro, E.; Giammaria, P.; La Barbera, A.; Lombardi, S.; Maraschi, L.; Stamerra, A.; Tavecchio, F.] INAF Natl Inst Astrophys, I-00136 Rome, Italy.
[Antoranz, P.; Da Vela, P.; Miranda, J. M.; Paoletti, R.] Univ Siena, I-53100 Siena, Italy.
[Antoranz, P.; Da Vela, P.; Miranda, J. M.; Paoletti, R.] INFN Pisa, I-53100 Siena, Italy.
[Babic, A.; Prester, D. Dominis; Gouinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Rijeka, Rudjer Boskov Inst, Croatian MAGIC Consortium, HR-10000 Zagreb, Croatia.
[Babic, A.; Prester, D. Dominis; Gouinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Split, HR-10000 Zagreb, Croatia.
[Banerjee, B.; Chatterjee, A.; Majumdar, P.] Saha Inst Nucl Phys, 1-AF Bidhannagar,Sect 1, Kolkata 700064, India.
[Barres de Almeida, U.] Ctr Brasileiro Pesquisas Fis CBPF MCTI, R Dr Xavier Sigaud 150 Urca, BR-22290180 Rio De Janeiro, RJ, Brazil.
[Barrio, J. A.; Bonnefoy, S.; Contreras, J. L.; Fidalgo, D.; Fonseca, M. V.; Lopez, M.; Rosillo, M. Nievas; Satalecka, K.; Scapin, V.] Univ Complutense, E-28040 Madrid, Spain.
[Becerra Gonzalez, J.; Clavero, R.; Colombo, E.; Garcia Lopez, J.; Herrera, J.; Manganaro, M.; Tescaro, D.; Will, M.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Becerra Gonzalez, J.; Clavero, R.; Colombo, E.; Garcia Lopez, J.; Herrera, J.; Manganaro, M.; Tescaro, D.; Will, M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Bednarek, W.; Idec, W.; Niedzwiecki, A.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Bernardini, E.] Humboldt Univ, Ist Phys, Newtonstr 15, D-12489 Berlin, Germany.
[Blanch, O.; Cortina, J.; Fernandez-Barral, A.; Gonzalez Munoz, A.; Guberman, D.; Lopez-Coto, R.; Lopez-Oramas, A.; Martinez, M.; Moralejo, A.; Palacio, J.; Rico, J.; Ward, J. E.] IFAE, Campus UAB, E-08193 Bellaterra, Spain.
[Bretz, T.; Dorner, D.; Elsaesser, D.; Glawion (Eisenacher), D.; Mannheim, K.; Steinbring, T.] Univ Wurzburg, D-97074 Wurzburg, Germany.
[Bretz, T.] Ecole Polytech Fed Lausanne, CH-1015 Lausanne, Switzerland.
[Carmona, E.; Delgado Mendez, C.] Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain.
[De Angelis, A.; Doro, M.; Mariotti, M.; Paiano, S.; Schultz, C.] Univ Padua, I-35131 Padua, Italy.
[De Angelis, A.; Doro, M.; Mariotti, M.; Paiano, S.; Schultz, C.] Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[de Ona Wilhelmi, E.; Wu, M. H.] CSIC, Inst Space Sci, IEEC, E-08193 Barcelona, Spain.
[Einecke, S.; Overkemping, A.; Rhode, W.; Thaele, J.] Tech Univ Dortmund, D-44221 Dortmund, Germany.
[Font, L.; Frantzen, K.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, E-08193 Bellaterra, Spain.
[Font, L.; Frantzen, K.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, E-08193 Bellaterra, Spain.
[Galindo, D.; Marcote, B.; Paredes, J. M.; Paredes-Fortuny, X.; Ribo, M.; Zanin, R.] Univ Barcelona, ICC, IEEC UB, E-08028 Barcelona, Spain.
[Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Mazin, D.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.; Teshima, M.] Univ Tokyo, ICRR, Japanese MAGIC Consortium, Tokyo 1138654, Japan.
[Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Mazin, D.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.; Teshima, M.] Kyoto Univ, Dept Phys, Kyoto 6068501, Japan.
[Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Mazin, D.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.; Teshima, M.] Kyoto Univ, Hakubi Ctr, Kyoto 6068501, Japan.
[Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Mazin, D.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.; Teshima, M.] Tokai Univ, Hiratsuka, Kanagawa 25912, Japan.
[Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Mazin, D.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.; Teshima, M.] Univ Tokushima, KEK, Tokushima, Japan.
[Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, SF-20500 Turku, Finland.
[Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Sillanpaa, A.; Takalo, L.] Univ Oulu, Dept Phys, SF-90100 Oulu, Finland.
[Lopez-Oramas, A.] CEA Saclay, IRFU, DSM, Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Makariev, M.; Maneva, G.; Temnikov, P.; Verguilov, V.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria.
[Nilsson, K.] Finnish Ctr Astron ESO FINCA, Turku, Finland.
[Persic, M.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy.
[Moroni, P. G. Prada; Shore, S. N.] Ist Nazl Fis Nucl, I-56126 Pisa, Italy.
[Prandini, E.] ISDC Sci Data Ctr Astrophys, CH-1290 Geneva, Switzerland.
[Torres, D. F.] ICREA, E-08193 Barcelona, Spain.
[Torres, D. F.] CSIC, Inst Space Sci, IEEC, E-08193 Barcelona, Spain.
[Treves, A.] Univ Insubria, I-22100 Como, Italy.
[Treves, A.] INFN Milano Bicocca, I-22100 Como, Italy.
[Boettcher, M.] North West Univ, Ctr Space Res, Private Bag X6001,Potchefstroom Campus, ZA-2520 Potchefstroom, South Africa.
[Villata, M.; Raiteri, C. M.; Carnerero, M. I.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy.
[Acosta-Pulido, J. A.; Carnerero, M. I.; Chinchilla, P.] Inst Astrofis Canarias, Tenerife, Spain.
[Acosta-Pulido, J. A.; Carnerero, M. I.; Chinchilla, P.] Univ La Laguna, Dept Astrofis, Tenerife, Spain.
[Bachev, R.; Ibryamov, S.; Semkov, E.; Strigachev, A.] Bulgarian Acad Sci, Inst Astron, 72 Tsarigradsko Shosse Blvd, BU-1784 Sofia, Bulgaria.
[Berdyugin, A.; Reinthal, R.] Tuorla Observ, Dept Phys & Astron, Vaisalantie 20, FI-21500 Piikkio, Finland.
[Blinov, D. A.; Grisinna, T. S.; Jorstad, S. G.; Joshi, M.; Kopatskaya, E. N.; Larionova, E. G.; Larionova, L. V.; Larionov, V. M.; Mokrushina, A. A.; Morozova, D. A.; Troitskaya, Yu. V.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, Univ Skij Pr 28, St Petersburg 198504, Russia.
[Blinov, D. A.] Univ Crete, Dept Phys, Iraklion 71003, Greece.
[Blinov, D. A.] Univ Crete, Inst Plasma Phys, Iraklion 71003, Greece.
[Blinov, D. A.] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Greece.
[Chen, W. P.; Eswaraiah, C.; Lin, H. C.] Natl Cent Univ, Grad Inst Astron, 300 Zhongda Rd, Zhongli 32001, Taiwan.
[Damljanovic, G.; Vince, O.] Astron Observ, Volgina 7, Belgrade 11060, Serbia.
[Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin, Ireland.
[Jorstad, S. G.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA.
[Kurtanidze, O. M.; Kurtanidze, S. O.; Nikolashvili, M. G.] Abastumani Observ, GA-0301 Abastumani, Rep of Georgia.
[Kurtanidze, O. M.] Kazan Fed Univ, Engelhardt Astron Observ, Kazan, Russia.
[Kurtanidze, O. M.] Guangzhou Univ, Ctr Astrophys, Guangzhou 510006, Guangdong, Peoples R China.
[Larionov, V. M.; Mokrushina, A. A.] Pulkovo Observ, St Petersburg, Russia.
[Latev, G.] Inst Astron, Sofia, Bulgaria.
[Latev, G.] NAO, Sofia, Bulgaria.
[Smith, P. S.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Barnes, J.] Salt Lake Community Coll, Dept Phys, Salt Lake City, UT 84070 USA.
[Guever, T.] Istanbul Univ, Fac Sci, Dept Astron & Space Sci, TR-34119 Istanbul, Turkey.
[Moody, J. W.] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA.
[Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80217 USA.
[Sun, S.] Fudan Univ, Ctr Field Theory & Particle Phys, Shanghai 200433, Peoples R China.
[Sun, S.] Fudan Univ, Dept Phys, Shanghai 200433, Peoples R China.
[Hovatta, T.; Lahteenmaki, A.; Tornikoski, M.; Tammi, J.; Ramakrishnan, V.] Aalto Univ, Metsahovi Radio Observ, Metsahovintie 114, FI-02540 Kylmala, Finland.
[Max-Moerbeck, W.] Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA.
[Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, POB 13000, FI-00076 Aalto, Finland.
[Angelakis, E.; Fuhrmann, L.; Myserlis, I.; Karamanavis, V.; Zensus, J. A.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Sievers, A.; Ungerechts, H.] Inst Radio Astron Milimetr, Ave Divina Pastora 7,Local 20, Granada 18012, Spain.
RP Balokovic, M (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.; Paneque, D (reprint author), Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.; Madejski, G; Chiang, J (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA.; Madejski, G; Chiang, J (reprint author), Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.; Furniss, A (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
EM mislavb@astro.caltech.edu; dpaneque@mppmu.mpg.de; madejski@stanford.edu;
amy.furniss@gmail.com; jchiang@slac.stanford.edu
RI Ramakrishnan, Venkatessh/C-8628-2017; Puljak, Ivica/D-8917-2017;
Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Larionov,
Valeri/H-1349-2013; Grishina, Tatiana/H-6873-2013; Miranda, Jose
Miguel/F-2913-2013; Blinov, Dmitry/G-9925-2013; Delgado,
Carlos/K-7587-2014; Torres, Diego/O-9422-2016; Barrio, Juan/L-3227-2014;
GAug, Markus/L-2340-2014; Cortina, Juan/C-2783-2017; Lahteenmaki,
Anne/L-5987-2013; Font, Lluis/L-4197-2014; Nieto, Daniel/J-7250-2015;
Poutanen, Juri/H-6651-2016; Contreras Gonzalez, Jose Luis/K-7255-2014;
Manganaro, Marina/B-7657-2011; Boggs, Steven/E-4170-2015; Lopez Moya,
Marcos/L-2304-2014; Temnikov, Petar/L-6999-2016; Maneva,
Galina/L-7120-2016; Makariev, Martin/M-2122-2016; Morozova,
Daria/H-1298-2013; Larionova, Elena/H-7287-2013
OI Karamanavis, Vassilis/0000-0003-3133-2617; Angelakis,
Emmanouil/0000-0001-7327-5441; Urry, Meg/0000-0002-0745-9792; de Ona
Wilhelmi, Emma/0000-0002-5401-0744; Bonnoli,
Giacomo/0000-0003-2464-9077; Prandini, Elisa/0000-0003-4502-9053;
Becerra Gonzalez, Josefa/0000-0002-6729-9022; Ramakrishnan,
Venkatessh/0000-0002-9248-086X; Villata, Massimo/0000-0003-1743-6946;
Pueschel, Elisa/0000-0002-0529-1973; Rana, Vikram/0000-0003-1703-8796;
Krause, Maria/0000-0001-7595-0914; Bird, Ralph/0000-0002-4596-8563;
Troitskiy, Ivan/0000-0002-4218-0148; Jorstad,
Svetlana/0000-0001-9522-5453; Larionov, Valeri/0000-0002-4640-4356;
Grishina, Tatiana/0000-0002-3953-6676; Miranda, Jose
Miguel/0000-0002-1472-9690; Blinov, Dmitry/0000-0003-0611-5784; Delgado,
Carlos/0000-0002-7014-4101; Torres, Diego/0000-0002-1522-9065; Barrio,
Juan/0000-0002-0965-0259; GAug, Markus/0000-0001-8442-7877; Cortina,
Juan/0000-0003-4576-0452; Font, Lluis/0000-0003-2109-5961; Nieto,
Daniel/0000-0003-3343-0755; Poutanen, Juri/0000-0002-0983-0049;
Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Manganaro,
Marina/0000-0003-1530-3031; Boggs, Steven/0000-0001-9567-4224; Lopez
Moya, Marcos/0000-0002-8791-7908; Temnikov, Petar/0000-0002-9559-3384;
Morozova, Daria/0000-0002-9407-7804; Larionova,
Elena/0000-0002-2471-6500
FU International Fulbright Science and Technology Award; NASA Headquarters
under the NASA Earth and Space Science Fellowship Program [NNX14AQ07H];
Department of Energy [DE-AC02-765F00515]; NASA [NNX13AO97G, NNG08FD60C,
NNX12AO90G, NNX14AQ58G]; French Space Agency (CNES); National
Aeronautics and Space Administration; U.S. Department of Energy Office
of Science; U.S. National Science Foundation; Smithsonian Institution;
NSERC in Canada; STFC in the U.K.; German BMBF; MPG; Italian INFN; INAF;
Swiss National Fund SNF; ERDF under the Spanish MINECO; Japanese JSPS;
MEXT; Centro de Excelencia Severo Ochoa [SEV-2012-0234, CPAN
CSD2007-00042]; Spanish Consolider-Ingenio programme [CSD2009-00064];
Academy of Finland [268740, 212656, 210338, 121148]; Croatian Science
Foundation (HrZZ) Project [09/176]; University of Rijeka [13.12.1.3.02];
DFG Collaborative Research Centers [SH3823/C4, SH3876/C3]; Polish MNiSzW
grant [745/N-HESS-MAGIC/2010/0]; Russian RFBR [15-02-00949]; St.
Petersburg University [6.38.335.2015]; South African Research Chairs
Initiative (SARChI) of the Department of Science and Technology;
National Research Foundation of South Africa; Institute of Astronomy and
Rozhen National Astronomical Observatory, Bulgaria Academy of Sciences;
Ministry of Education, Science, and Technological Development of the
Republic of Serbia [176011, 176004, 176021]; Scientific Research Fund of
the Bulgarian Ministry of Education and Sciences [DO 02-137
(BIn-13/09)]; Shota Rustaveli National Science Foundation
[FR/638/6-320/12, 31/77]; Istanbul University [49429, 48285]; Bilim
Akademisi (BAGEP program); TUBITAK [13AT100-431, 13AT100-466,
13AT60-430]; NASA grants [NNX08AW31G, NNX11A043G]; NSF grants
[AST-0808050, AST-1109911]
FX M.B. acknowledges support from the International Fulbright Science and
Technology Award, and from NASA Headquarters under the NASA Earth and
Space Science Fellowship Program, grant NNX14AQ07H. This research was
supported in part by the Department of Energy Contract DE-ACO2-765F00515
to the SLAC National Accelerator Center. G.M. and A.F. acknowledge the
support via NASA grant NNX13AO97G. D.B. acknowledges support from the
French Space Agency (CNES) for financial support.; This work was
supported under NASA Contract No. NNG08FD60C and made use of data from
the NuSTAR mission, a project led by the California Institute of
Technology, managed by the Jet Propulsion Laboratory, and funded by the
National Aeronautics and Space Administration. We thank the NuSTAR
Operations, Software, and Calibration teams for support with the
execution and analysis of these observations. This research has made use
of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by
the ASI Science Data Center (ASDC, Italy) and the California Institute
of Technology (USA).; VERITAS is supported by grants from the U.S.
Department of Energy Office of Science, the U.S. National Science
Foundation, and the Smithsonian Institution, by NSERC in Canada, and by
STFC in the U.K. We acknowledge the excellent work of the technical
support staff at the Fred Lawrence Whipple Observatory and at the
collaborating institutions in the construction and operation of the
instrument. The VERITAS Collaboration is grateful to Trevor Weekes for
his seminal contributions and leadership in the field of VHE gamma-ray
astrophysics, which made this study possible.; The MAGIC Collaboration
would like to thank the Institute de Astrofisica de Canarias for the
excellent working conditions at the Observatorio del Roque de los
Muchachos in La Palma. The financial support of the German BMBF and MPG,
the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under
the Spanish MINECO, and the Japanese JSPS and MEXT is gratefully
acknowledged. This work was also supported by the Centro de Excelencia
Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark
CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme,
by grant 268740 of the Academy of Finland, by the Croatian Science
Foundation (HrZZ) Project 09/176 and the University of Rijeka Project
13.12.1.3.02, by the DFG Collaborative Research Centers SH3823/C4 and
SH3876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.; The
St. Petersburg University team acknowledges support from Russian RFBR
grant 15-02-00949 and St. Petersburg University research grant
6.38.335.2015.; The work of M.B. is supported by the South African
Research Chairs Initiative (SARChI) of the Department of Science and
Technology and the National Research Foundation of South Africa. Any
opinion, finding, and conclusion or recommendation expressed in this
material is that of the authors and the NRF does not accept any
liability in this regard.; G.D. and O.V. gratefully acknowledge the
observing grant support from the Institute of Astronomy and Rozhen
National Astronomical Observatory, Bulgaria Academy of Sciences. This
work is a part of the Projects No. 176011 (Dynamics and kinematics of
celestial bodies and systems), No. 176004 (Stellar physics), and No.
176021 (Visible and invisible matter in nearby galaxies: theory and
observations) supported by the Ministry of Education, Science, and
Technological Development of the Republic of Serbia.; This research was
partially supported by the Scientific Research Fund of the Bulgarian
Ministry of Education and Sciences under grant DO 02-137 (BIn-13/09).;
The Abastumani team acknowledges financial support of the project
FR/638/6-320/12 by the Shota Rustaveli National Science Foundation under
contract 31/77.; T.G. acknowledges support from Istanbul University
(Project numbers 49429 and 48285), Bilim Akademisi (BAGEP program), and
TUBITAK (project numbers 13AT100-431, 13AT100-466, and 13AT60-430).; The
Boston University effort was supported in part by NASA grants NNX12AO90G
and NNX14AQ58G.; The OVRO 40 m monitoring program is supported in part
by NASA grants NNX08AW31G and NNX11A043G and NSF grants AST-0808050 and
AST-1109911.; The Metsahovi team acknowledges the support from the
Academy of Finland to our observing projects (numbers 212656, 210338,
121148, and others).
NR 120
TC 9
Z9 9
U1 7
U2 20
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 156
DI 10.3847/0004-637X/819/2/156
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700068
ER
PT J
AU Dorodnitsyn, A
Kallman, T
Proga, D
AF Dorodnitsyn, A.
Kallman, T.
Proga, D.
TI PARSEC-SCALE ACCRETION AND WINDS IRRADIATED BY A QUASAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; galaxies: active; galaxies: Seyfert;
radiation: dynamics
ID ACTIVE GALACTIC NUCLEI; ABSORPTION-LINE QUASARS; X-RAY BINARIES;
RADIATIVE-TRANSFER; SEYFERT-GALAXIES; OBSCURING TORUS; BLACK-HOLES;
MAGNETIZED DISKS; ANGULAR-MOMENTUM; CIRCINUS GALAXY
AB We present numerical simulations of properties of a parsec-scale torus exposed to illumination by the central black hole in an active galactic nucleus (AGN). Our physical model allows to investigate the balance between the formation of winds and accretion simultaneously. Radiation-driven winds are allowed by taking into account radiation pressure due to UV and IR radiation along with X-ray heating and dust sublimation. Accretion is allowed through angular momentum transport and the solution of the equations of radiative, viscous radiation hydrodynamics. Our methods adopt flux-limited diffusion radiation hydrodynamics for the dusty, infrared pressure driven part of the flow, along with X-ray heating and cooling. Angular momentum transport in the accreting part of the flow is modeled using effective viscosity. Our results demonstrate that radiation pressure on dust can play an important role in shaping AGN obscuration. For example, when the luminosity illuminating the torus exceeds L > 0.01 L-Edd, where L-Edd is the Eddington luminosity, we find no episodes of sustained disk accretion because radiation pressure does not allow a disk to form. Despite the absence of the disk accretion, the flow of gas to smaller radii still proceeds at a rate 10(-4)-10(-1)M(circle dot) yr(-1). through the capturing of the gas from the hot evaporative flow, thus providing a mechanism to deliver gas from a radiation-pressure dominated torus to the inner accretion disk. As L/L-edd increases, larger radiation input leads to larger torus aspect ratios and increased obscuration of the central black hole. We also find the important role of the X-ray heated gas in shaping the obscuring torus.
C1 [Dorodnitsyn, A.; Kallman, T.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA.
[Dorodnitsyn, A.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA.
[Dorodnitsyn, A.] Space Res Inst, Profsoyuznaya St 84-32, Moscow 117997, Russia.
[Proga, D.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
RP Dorodnitsyn, A (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA.; Dorodnitsyn, A (reprint author), Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA.; Dorodnitsyn, A (reprint author), Space Res Inst, Profsoyuznaya St 84-32, Moscow 117997, Russia.
FU NASA [10-ATP10-0171, NNX11AI96G]
FX This work was supported by NASA under Astrophysics Theory Program grants
10-ATP10-0171 and NNX11AI96G.
NR 90
TC 4
Z9 4
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 115
DI 10.3847/0004-637X/819/2/115
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700027
ER
PT J
AU Fortenberry, RC
Francisco, JS
Lee, TJ
AF Fortenberry, Ryan C.
Francisco, Joseph S.
Lee, Timothy J.
TI TOWARD THE ASTRONOMICAL DETECTION OF THE PROTON-BOUND COMPLEX NN-HCO+:
IMPLICATIONS FOR THE SPECTRA OF PROTOPLANETARY DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: lines and bands; ISM: molecules; molecular data;
protoplanetary disks
ID QUARTIC FORCE-FIELDS; VIBRATIONAL FREQUENCIES; SPECTROSCOPIC CONSTANTS;
BASIS-SETS; INTERSTELLAR; ABUNDANCE; CATION; LINE; ISOTOPOLOGUES;
U93.174
AB Proton-bound complexes have been hypothesized as further means of detecting the nitrogen molecule in the interstellar medium. The study of such complexes has largely been hindered by the necessary experimental setups utilized or by their difficulty in producing and/or analyzing computed potential energy surfaces. Here the NN-HCO+ proton-bound complex is analyzed via quartic force fields (QFFs). While QFFs have produced meaningful results for other proton-bound complexes, they have been hindered by double-well potentials or flat potential surfaces. NN-HCO+ is not affected by these constraints. This strongly dipolar (3.63 D) molecule can be observed rotationally unlike the more heavily analyzed OCHCO+ and NNHNN+ proton-bound complexes. Additionally, the large absorption feature corresponding to the proton motion, a hallmark of proton-bound complexes, is much higher in frequency at 2547.1 cm(-1), changing the range of experimental observation for the bright frequency. NN-HCO+ is hypothesized to be present in protoplanetary disks where N2H+ and CO are known. As such, it may help to influence the nitrogen budget of planet-forming astronomical regions.
C1 [Fortenberry, Ryan C.] Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA.
[Francisco, Joseph S.] Univ Nebraska, Dept Chem, Lincoln, NE 68588 USA.
[Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Fortenberry, RC (reprint author), Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA.
EM rfortenberry@georgiasouthern.edu
RI Lee, Timothy/K-2838-2012
FU Georgia Southern University; National Aeronautics and Space
Administration through the NASA Astrobiology Institute [NNH13ZDA017C]
FX R.C.F. wishes to acknowledge Georgia Southern University for providing
start-up funds utilized in this work. This material is based upon work
supported by the National Aeronautics and Space Administration through
the NASA Astrobiology Institute under Cooperative Agreement Notice
NNH13ZDA017C issued through the Science Mission Directorate. The CheMVP
program developed at the Center for Computational Quantum Chemistry at
University of Georgia was used to create Figure 1. The authors would
like to acknowledge Prof. T. Daniel Crawford of Virginia Tech for the
use of the computer hardware necessary to perform the computations in
this project.
NR 45
TC 3
Z9 3
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 141
DI 10.3847/0004-637X/819/2/141
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700053
ER
PT J
AU Furst, F
Muller, C
Madsen, KK
Lanz, L
Rivers, E
Brightman, M
Arevalo, P
Balokovic, M
Beuchert, T
Boggs, SE
Christensen, FE
Craig, WW
Dauser, T
Farrah, D
Graefe, C
Hailey, CJ
Harrison, FA
Kadler, M
King, A
Krauss, F
Madejski, G
Matt, G
Marinucci, A
Markowitz, A
Ogle, P
Ojha, R
Rothschild, R
Stern, D
Walton, DJ
Wilms, J
Zhang, W
AF Fuerst, F.
Mueller, C.
Madsen, K. K.
Lanz, L.
Rivers, E.
Brightman, M.
Arevalo, P.
Balokovic, M.
Beuchert, T.
Boggs, S. E.
Christensen, F. E.
Craig, W. W.
Dauser, T.
Farrah, D.
Graefe, C.
Hailey, C. J.
Harrison, F. A.
Kadler, M.
King, A.
Krauss, F.
Madejski, G.
Matt, G.
Marinucci, A.
Markowitz, A.
Ogle, P.
Ojha, R.
Rothschild, R.
Stern, D.
Walton, D. J.
Wilms, J.
Zhang, W.
TI NuSTAR AND XMM-NEWTON OBSERVATIONS OF THE HARD X- RAY SPECTRUM OF
CENTAURUS A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (Centaurus A); X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; RADIO GALAXY CENTAURUS; PHOTON IMAGING CAMERA;
CLUMPY-TORUS MODELS; COMPTON-THICK; 3C 273; BEPPOSAX OBSERVATIONS;
INTERSTELLAR-MEDIUM; CORONAL PROPERTIES; SEYFERT-GALAXIES
AB We present simultaneous XMM-Newton and Nuclear Spectroscopic Telescope Array (NuSTAR) observations spanning 3-78 keV of the nearest radio galaxy, Centaurus. A (Cen A). The accretion geometry around the central engine in Cen. A is still debated, and we investigate possible configurations using detailed X-ray spectral modeling. NuSTAR imaged the central region of Cen. A with subarcminute resolution at X-ray energies above 10 keV for the first time, but found no evidence for an extended source or other off-nuclear point sources. The XMM-Newton and NuSTAR spectra agree well and can be described with an absorbed power law with a photon index Gamma = 1.815 +/- 0.005 and a fluorescent Fe K alpha line in good agreement with literature values. The spectrum does not require a high-energy exponential rollover, with a constraint of E-fold > 1 MeV. A thermal Comptonization continuum describes the data well, with parameters that agree with values measured by INTEGRAL, in particular an electron temperature kT(e) between approximate to 100-300 keV and seed photon input temperatures between 5 and 50 eV. We do not find evidence for reflection or a broad iron line and put stringent upper limits of R < 0.01 on the reflection fraction and accretion disk illumination. We use archival Chandra data to estimate the contribution from diffuse emission, extra-nuclear point sources, and the outer X-ray jet to the observed NuSTAR and XMM-Newton X-ray spectra and find the contribution to be negligible. We discuss different scenarios for the physical origin of the observed hard X-ray spectrum and conclude that the inner disk is replaced by an advection-dominated accretion flow or that the X-rays are dominated by synchrotron self-Compton emission from the inner regions of the radio jet or a combination thereof.
C1 [Fuerst, F.; Madsen, K. K.; Rivers, E.; Brightman, M.; Balokovic, M.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Mueller, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Mueller, C.; Beuchert, T.; Graefe, C.; Kadler, M.; Krauss, F.] Univ Wurzburg, Lehrstuhl Astron, D-97074 Wurzburg, Germany.
[Mueller, C.; Beuchert, T.; Dauser, T.; Graefe, C.; Krauss, F.; Wilms, J.] Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany.
[Mueller, C.; Beuchert, T.; Dauser, T.; Graefe, C.; Krauss, F.; Wilms, J.] ECAP, D-96049 Bamberg, Germany.
[Lanz, L.; Ogle, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile.
[Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[King, A.; Madejski, G.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[Matt, G.; Marinucci, A.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Markowitz, A.; Rothschild, R.] Univ Calif San Diego, CASS, La Jolla, CA 92093 USA.
[Ojha, R.; Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ojha, R.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Ojha, R.] Catholic Univ Amer, Washington, DC 20064 USA.
[Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Furst, F (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RI Wilms, Joern/C-8116-2013; Boggs, Steven/E-4170-2015;
OI Wilms, Joern/0000-0003-2065-5410; Boggs, Steven/0000-0001-9567-4224;
Krauss, Felicia/0000-0001-6191-1244; Kadler,
Matthias/0000-0001-5606-6154
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; ESA
Member States; Bundesministerium fur Wirtschaft und Technologie (BMWi)
through Deutsches Zentrum fur Luft- und Raumfahrt (DLR) [50OR1404];
Deutsche Forschungsgemeinschaft (DFG) [Wi 1860 10-1]; NASA through Fermi
Guest Investigator grants [NNH09ZDA001N, NNH10ZDA001N, NNH12ZDA001N,
NNH13ZDA001N-FERMI]; NASA Headquarters under the NASA Earth and Space
Science Fellowship Program [NNX14AQ07H]
FX We thank the anonymous referee for comments that helped to improve this
work. This work was supported under NASA Contract No. NNG08FD60C and
made use of data from the NuSTAR mission, a project led by the
California Institute of Technology, managed by the Jet Propulsion
Laboratory, and funded by the National Aeronautics and Space
Administration. We thank the NuSTAR Operations, Software, and
Calibration teams for support with the execution and analysis of these
observations. This research has made use of the NuSTAR Data Analysis
Software (NuSTARDAS), jointly developed by the ASI Science Data Center
(ASDC, Italy) and the California Institute of Technology (USA). Based on
observations obtained with XMM-Newton, an ESA science mission with
instruments and contributions directly funded by ESA Member States and
NASA. This research has made use of a collection of ISIS scripts
provided by the Dr. Karl Remeis Observatory, Bamberg, Germany at
http://www.sternwarte.uni-erlangen.de/isis/. C.M. acknowledges the
support of the Bundesministerium fur Wirtschaft und Technologie (BMWi)
through Deutsches Zentrum fur Luft- und Raumfahrt (DLR) grant 50OR1404.
We acknowledge support of the Deutsche Forschungsgemeinschaft (DFG)
through grant Wi 1860 10-1. This research was funded in part by NASA
through Fermi Guest Investigator grants NNH09ZDA001N, NNH10ZDA001N,
NNH12ZDA001N, NNH13ZDA001N-FERMI. This research was supported by an
appointment to the NASA Postdoctoral Program at the Goddard Space Flight
Center, administered by Oak Ridge Associated Universities through a
contract with NASA. M.B. acknowledges support from NASA Headquarters
under the NASA Earth and Space Science Fellowship Program, grant
NNX14AQ07H. We would like to thank John E. Davis for the slxfig module,
which was used to produce all figures in this work.
NR 83
TC 4
Z9 4
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 150
DI 10.3847/0004-637X/819/2/150
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700062
ER
PT J
AU Guerrero, G
Smolarkiewicz, PK
Dal Pino, EMD
Kosovichev, AG
Mansour, NN
AF Guerrero, G.
Smolarkiewicz, P. K.
de Gouveia Dal Pino, E. M.
Kosovichev, A. G.
Mansour, N. N.
TI ON THE ROLE OF TACHOCLINES IN SOLAR AND STELLAR DYNAMOS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: activity; stars: interiors; stars: magnetic field; Sun: interior;
Sun: magnetic fields; Sun: rotation
ID LARGE-EDDY SIMULATIONS; DIFFERENTIAL ROTATION; MERIDIONAL CIRCULATION;
CONVECTIVE DYNAMO; TOROIDAL FIELDS; MAGNETIC CYCLES; STARS; TRANSPORT;
FLUX; INSTABILITY
AB Rotational shear layers at the boundary between radiative and convective zones, tachoclines, play a key role in the process of magnetic field generation in solar-like stars. We present two sets of global simulations of rotating turbulent convection and dynamo. The first set considers a stellar convective envelope only; the second one, aiming at the formation of a tachocline, also considers the upper part of the radiative zone. Our results indicate that the resulting properties of the mean flows and dynamo, such as the growth rate, saturation energy, and mode, depend on the Rossby number (Ro). For the first set of models either oscillatory (with similar to 2 yr period) or steady dynamo solutions are obtained. The models in the second set naturally develop a tachocline, which in turn leads to the generation of a strong mean magnetic field. Since the field is also deposited in the stable deeper layer, its evolutionary timescale is much longer than in the models without a tachocline. Surprisingly, the magnetic field in the upper turbulent convection zone evolves on the same timescale as the deep field. These models result in either an oscillatory dynamo with a similar to 30 yr period or a steady dynamo depending on Ro. In terms of the mean-field dynamo coefficients computed using the first-order smoothing approximation, the field evolution in the oscillatory models without a tachocline seems to be consistent with dynamo waves propagating according to the Parker-Yoshimura sign rule. In the models with tachoclines the dynamics is more complex and involves other transport mechanisms as well as tachocline instabilities.
C1 [Guerrero, G.] Univ Fed Minas Gerais, Dept Phys, Ave Antonio Carlos 6627, BR-31270901 Belo Horizonte, MG, Brazil.
[Smolarkiewicz, P. K.] European Ctr Medium Range Weather Forecasts, Shinfield Pk, Reading RG2 9AX, Berks, England.
[de Gouveia Dal Pino, E. M.] Univ Sao Paulo, IAG, Dept Astron, Rua Mato 1226, BR-05508090 Sao Paulo, SP, Brazil.
[Kosovichev, A. G.] New Jersey Inst Technol, Newark, NJ 07103 USA.
[Mansour, N. N.] NASA, Ames Res Ctr, Mountain View, CA 94040 USA.
RP Guerrero, G (reprint author), Univ Fed Minas Gerais, Dept Phys, Ave Antonio Carlos 6627, BR-31270901 Belo Horizonte, MG, Brazil.; Smolarkiewicz, PK (reprint author), European Ctr Medium Range Weather Forecasts, Shinfield Pk, Reading RG2 9AX, Berks, England.; Dal Pino, EMD (reprint author), Univ Sao Paulo, IAG, Dept Astron, Rua Mato 1226, BR-05508090 Sao Paulo, SP, Brazil.; Kosovichev, AG (reprint author), New Jersey Inst Technol, Newark, NJ 07103 USA.; Mansour, NN (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94040 USA.
EM guerrero@fisica.ufmg.br; smolar@ecmwf.int; dalpino@astro.iag.usp.br;
sasha@bbso.njit.edu; Nagi.N.Mansour@nasa.gov
RI de Gouveia Dal Pino, Elisabete/H-9560-2013
OI de Gouveia Dal Pino, Elisabete/0000-0001-8058-4752
FU FAPESP [2013/11679-4, 2013/10559-5, 2009/54006-4]; CNPq [306598/2009-4];
NASA [NNX09AJ85g, NNX14AB70G]; European Research Council under the
European Union's Seventh Framework Programme (FP7/ERC) [320375]
FX We thank the anonymous referee for comments and suggestions on the
manuscript. This work was partly funded by FAPESP grants 2013/11679-4
(G.G.) and 2013/10559-5 (E.M.G.D.P.), CNPq grant 306598/2009-4
(E.M.G.D.P.), and NASA grants NNX09AJ85g and NNX14AB70G. G.G. also
thanks CNPq for travel support. P.K.S. is supported by funding received
from the European Research Council under the European Union's Seventh
Framework Programme (FP7/2012/ERC Grant agreement no. 320375). The
simulations were performed in the NASA cluster Pleiades and the
computing facilities of the Laboratory of Astroinformatics (IAG/USP,
NAT/Unicsul) supported by a FAPESP (grant 2009/54006-4).
NR 44
TC 6
Z9 6
U1 3
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 104
DI 10.3847/0004-637X/819/2/104
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700016
ER
PT J
AU Lam, MT
Cordes, JM
Chatterjee, S
Arzoumanian, Z
Crowter, K
Demorest, PB
Dolch, T
Ellis, JA
Ferdman, RD
Fonseca, EF
Gonzalez, ME
Jones, G
Jones, ML
Levin, L
Madison, DR
McLaughlin, MA
Nice, DJ
Pennucci, TT
Ransom, SM
Siemens, X
Stairs, IH
Stovall, K
Swiggum, JK
Zhu, WW
AF Lam, M. T.
Cordes, J. M.
Chatterjee, S.
Arzoumanian, Z.
Crowter, K.
Demorest, P. B.
Dolch, T.
Ellis, J. A.
Ferdman, R. D.
Fonseca, E. F.
Gonzalez, M. E.
Jones, G.
Jones, M. L.
Levin, L.
Madison, D. R.
McLaughlin, M. A.
Nice, D. J.
Pennucci, T. T.
Ransom, S. M.
Siemens, X.
Stairs, I. H.
Stovall, K.
Swiggum, J. K.
Zhu, W. W.
TI THE NANOGRAV NINE-YEAR DATA SET: NOISE BUDGET FOR PULSAR ARRIVAL TIMES
ON INTRADAY TIMESCALES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational waves; pulsars: general
ID MILLISECOND PULSARS; WIDE-BAND; INTERSTELLAR SCINTILLATION; RADIO
PULSARS; PRECISION; DISPERSION; PROPAGATION; J1713+0747; PRECESSION;
STABILITY
AB The use of pulsars as astrophysical clocks for gravitational wave (GW) experiments demands the highest possible timing precision. Pulse times of arrival (TOAs) are limited by stochastic processes that occur in the pulsar itself, along the line of sight through the interstellar medium, and in the measurement process. On timescales of seconds to hours, the TOA variance exceeds that from template-fitting errors due to additive noise. We assess contributions to the total variance from two additional effects: amplitude and phase jitter intrinsic to single pulses and changes in the interstellar impulse response from scattering. The three effects have different dependencies on time, frequency, and pulse signal-to-noise ratio. We use data on 37 pulsars from the North American Nanohertz Observatory for GWs to assess the individual contributions to the overall intraday noise budget for each pulsar. We detect jitter in 22 pulsars and estimate the average value of rms jitter in our pulsars to be similar to 1% of pulse phase. We examine how jitter evolves as a function of frequency and find evidence for evolution. Finally, we compare our measurements with previous noise parameter estimates and discuss methods to improve GW detection pipelines.
C1 [Lam, M. T.; Cordes, J. M.; Chatterjee, S.; Dolch, T.; Madison, D. R.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Lam, M. T.; Cordes, J. M.; Chatterjee, S.; Dolch, T.; Madison, D. R.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
[Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Code 662, Greenbelt, MD 20771 USA.
[Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA.
[Crowter, K.; Fonseca, E. F.; Gonzalez, M. E.; Stairs, I. H.; Zhu, W. W.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
[Demorest, P. B.] Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA.
[Dolch, T.] Hillsdale Coll, Dept Phys, 33 E Coll St, Hillsdale, MI 49242 USA.
[Ellis, J. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Ferdman, R. D.; Stairs, I. H.] McGill Space Inst, 3550 Univ, Montreal, PQ H3A 2A7, Canada.
[Gonzalez, M. E.] Vancouver Coastal Hlth Author, Dept Nucl Med, Vancouver, BC V5Z 1M9, Canada.
[Jones, G.; Pennucci, T. T.] Columbia Univ, Dept Phys, 550 120th St, New York, NY 10027 USA.
[Jones, M. L.; Levin, L.; McLaughlin, M. A.; Swiggum, J. K.] Univ Virginia, Dept Phys, POB 6315, Morgantown, WV 26505 USA.
[Levin, L.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Madison, D. R.; Ransom, S. M.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
[Nice, D. J.] Lafayette Coll, Dept Phys, Easton, PA 18042 USA.
[Pennucci, T. T.] Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA.
[Siemens, X.; Swiggum, J. K.] Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, POB 413, Milwaukee, WI 53201 USA.
[Stovall, K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
[Zhu, W. W.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
RP Lam, MT (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.; Lam, MT (reprint author), Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
EM mlam@astro.cornell.edu
FU NSF PIRE program [0968296]; NSF Physics Frontier Center award [1430284];
NSERC Discovery Grant and Discovery Accelerator Supplement; Canadian
Institute for Advanced Research; NASA New York Space Grant [NNX15AK07H];
NASA through Einstein Fellowship [PF3-140116]; National Aeronautics and
Space Administration
FX We would like to thank Michael Jones for useful discussions on
statistical methods. The NANOGrav Project receives support from NSF PIRE
program award number 0968296 and NSF Physics Frontier Center award
number 1430284. NANOGrav research at UBC is supported by an NSERC
Discovery Grant and Discovery Accelerator Supplement and the Canadian
Institute for Advanced Research. MTL acknowledges partial support by
NASA New York Space Grant award number NNX15AK07H. JAE acknowledges
support by NASA through Einstein Fellowship grant PF3-140116. Portions
of this research were carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. TTP was a student at the National
Radio Astronomy Observatory (NRAO) while this project was undertaken.
Data for the project were collected using the facilities of the NRAO and
the Arecibo Observatory. The NRAO is a facility of the NSF operated
under cooperative agreement by Associated Universities, Inc. The Arecibo
Observatory is operated by SRI International under a cooperative
agreement with the NSF (AST-1100968), and in alliance with the Ana G.
Mendez-Universidad Metropolitana, and the Universities Space Research
Association.
NR 66
TC 1
Z9 1
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 155
DI 10.3847/0004-637X/819/2/155
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700067
ER
PT J
AU Street, RA
Udalski, A
Novati, SC
Hundertmark, MPG
Zhu, W
Gould, A
Yee, J
Tsapras, Y
Bennett, DP
Jorgensen, UG
Dominik, M
Andersen, MI
Bachelet, E
Bozza, V
Bramich, DM
Burgdorf, MJ
Cassan, A
Ciceri, S
D'Ago, G
Dong, SB
Evans, DF
Gu, SH
Harkonnen, H
Hinse, TC
Horne, K
Jaimes, RF
Kains, N
Kerins, E
Korhonen, H
Kuffmeier, M
Mancini, L
Menzies, J
Mao, S
Peixinho, N
Popovas, A
Rabus, M
Rahvar, S
Ranc, C
Rasmussen, RT
Scarpetta, G
Schmidt, R
Skottfelt, J
Snodgrass, C
Southworth, J
Steele, IA
Surdej, J
Unda-Sanzana, E
Verma, P
von Essen, C
Wambsganss, J
Wang, YB
Wertz, O
Poleski, R
Pawlak, M
Szymanski, MK
Skowron, J
Mroz, P
Kozlowski, S
Wyrzykowski, L
Pietrukowicz, P
Pietrzynski, G
Soszynski, I
Ulaczyk, K
Beichman, C
Bryden, G
Carey, S
Gaudi, BS
Henderson, CB
Pogge, RW
Shvartzvald, Y
Abe, F
Asakura, Y
Bhattacharya, A
Bond, IA
Donachie, M
Freeman, M
Fukui, A
Hirao, Y
Inayama, K
Itow, Y
Koshimoto, N
Li, MCA
Ling, CH
Masuda, K
Matsubara, Y
Muraki, Y
Nagakane, M
Nishioka, T
Ohnishi, K
Oyokawa, H
Rattenbury, N
Saito, T
Sharan, A
Sullivan, DJ
Sumi, T
Suzuki, D
Tristram, J
Wakiyama, Y
Yonehara, A
Han, C
Choi, JY
Park, H
Jung, YK
Shin, IG
AF Street, R. A.
Udalski, A.
Novati, S. Calchi
Hundertmark, M. P. G.
Zhu, W.
Gould, A.
Yee, J.
Tsapras, Y.
Bennett, D. P.
Jorgensen, U. G.
Dominik, M.
Andersen, M. I.
Bachelet, E.
Bozza, V.
Bramich, D. M.
Burgdorf, M. J.
Cassan, A.
Ciceri, S.
D'Ago, G.
Dong, Subo
Evans, D. F.
Gu, Sheng-Hong
Harkonnen, H.
Hinse, T. C.
Horne, Keith
Jaimes, R. Figuera
Kains, N.
Kerins, E.
Korhonen, H.
Kuffmeier, M.
Mancini, L.
Menzies, J.
Mao, S.
Peixinho, N.
Popovas, A.
Rabus, M.
Rahvar, S.
Ranc, C.
Rasmussen, R. Tronsgaard
Scarpetta, G.
Schmidt, R.
Skottfelt, J.
Snodgrass, C.
Southworth, J.
Steele, I. A.
Surdej, J.
Unda-Sanzana, E.
Verma, P.
Von Essen, C.
Wambsganss, J.
Wang, Yi-Bo
Wertz, O.
Poleski, R.
Pawlak, M.
Szymanski, M. K.
Skowron, J.
Mroz, P.
Kozlowski, S.
Wyrzykowski, L.
Pietrukowicz, P.
Pietrzynski, G.
Soszynski, I.
Ulaczyk, K.
Beichman, C.
Bryden, G.
Carey, S.
Gaudi, B. S.
Henderson, C. B.
Pogge, R. W.
Shvartzvald, Y.
Abe, F.
Asakura, Y.
Bhattacharya, A.
Bond, I. A.
Donachie, M.
Freeman, M.
Fukui, A.
Hirao, Y.
Inayama, K.
Itow, Y.
Koshimoto, N.
Li, M. C. A.
Ling, C. H.
Masuda, K.
Matsubara, Y.
Muraki, Y.
Nagakane, M.
Nishioka, T.
Ohnishi, K.
Oyokawa, H.
Rattenbury, N.
Saito, To
Sharan, A.
Sullivan, D. J.
Sumi, T.
Suzuki, D.
Tristram, J.
Wakiyama, Y.
Yonehara, A.
Han, C.
Choi, J-Y.
Park, H.
Jung, Y. K.
Shin, I-G.
CA RoboNet Project
MiNDSTEp Consortium
OGLE Project
Spitzer Team
MOA Collaboration
KMTNet Modeling Team
TI SPITZER PARALLAX OF OGLE-2015-BLG-0966: A COLD NEPTUNE IN THE GALACTIC
DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing: micro
ID GRAVITATIONAL LENSING EXPERIMENT; MAGNIFICATION MICROLENSING EVENTS;
DIFFERENCE IMAGE-ANALYSIS; SATELLITE MASS; OGLE-III; PLANETS;
PHOTOMETRY; STARS; BULGE; TELESCOPE
AB We report the detection of a cold Neptune m(planet) = 21 +/- 2M(circle plus) orbiting a 0.38M(circle dot) M dwarf lying 2.5-3.3 kpc toward the Galactic center as part of a campaign combining ground-based and Spitzer observations to measure the Galactic distribution of planets. This is the first time that the complex real-time protocols described by Yee et al., which aim to maximize planet sensitivity while maintaining sample integrity, have been carried out in practice. Multiple survey and follow. up teams successfully combined their efforts within the framework of these protocols to detect this planet. This is the second planet in the Spitzer Galactic distribution sample. Both are in the near. to. mid-disk and are clearly not in the Galactic bulge.
C1 [Street, R. A.; Bachelet, E.] LCOGT, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
[Udalski, A.; Poleski, R.; Pawlak, M.; Szymanski, M. K.; Skowron, J.; Mroz, P.; Kozlowski, S.; Wyrzykowski, L.; Pietrukowicz, P.; Pietrzynski, G.; Soszynski, I.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland.
[Novati, S. Calchi; Beichman, C.] CALTECH, NASA Exoplanet Sci Inst, MS 100-22, Pasadena, CA 91125 USA.
[Novati, S. Calchi; Bozza, V.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo 2 132, I-84084 Fisciano, Italy.
[Novati, S. Calchi; D'Ago, G.; Scarpetta, G.; Verma, P.] IIASS, Via G Pellegrino 19, I-84019 Vietri Sul Mare, SA, Italy.
[Hundertmark, M. P. G.; Jorgensen, U. G.; Harkonnen, H.; Kuffmeier, M.; Popovas, A.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Hundertmark, M. P. G.; Jorgensen, U. G.; Harkonnen, H.; Kuffmeier, M.; Popovas, A.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Gould, A.; Poleski, R.; Gaudi, B. S.; Henderson, C. B.; Pogge, R. W.] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA.
[Yee, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Tsapras, Y.; Schmidt, R.; Wambsganss, J.] Univ Heidelberg ZAH, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Bennett, D. P.; Bhattacharya, A.; Wakiyama, Y.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Dominik, M.; Horne, Keith; Jaimes, R. Figuera] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Andersen, M. I.; Korhonen, H.] Univ Copenhagen, Niels Bohr Inst, Juliane Mariesvej 30, DK-2100 Copenhagen O, Denmark.
[Andersen, M. I.; Korhonen, H.] Univ Copenhagen, Dark Cosmol Ctr, Juliane Mariesvej 30, DK-2100 Copenhagen O, Denmark.
[Bachelet, E.; Bramich, D. M.] Qatar Fdn, Qatar Environm & Energy Res Inst, POB 5825, Doha, Qatar.
[Bozza, V.] Inst Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Burgdorf, M. J.] Univ Hamburg, Meteorol Inst, Bundesstr 55, D-20146 Hamburg, Germany.
[Cassan, A.; Ranc, C.] Univ Paris 06, Sorbonne Univ, 98 Bis bd Arago, F-75014 Paris, France.
[Cassan, A.; Ranc, C.] CNRS, UMR 7095, Inst Astrophys Paris, 98 Bis bd Arago, F-75014 Paris, France.
[Ciceri, S.; Mancini, L.; Rabus, M.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Yi He Yuan Rd 5, Beijing 100871, Peoples R China.
[Evans, D. F.; Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Gu, Sheng-Hong; Wang, Yi-Bo] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China.
[Hinse, T. C.] Korea Astron & Space Sci Inst, 776 Daedukdae Ro, Daejeon 305348, South Korea.
[Jaimes, R. Figuera] European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Kains, N.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Korhonen, H.] ESO FINCA, Finnish Ctr Astron, Vaisalantie 20, FI-21500 Piikkio, Finland.
[Menzies, J.] S African Astron Observ, POB 9, ZA-7935 Observatory, South Africa.
[Mao, S.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Peixinho, N.; Unda-Sanzana, E.] Univ Antofagasta, Fac Ciencias Basicas, Unidad Astron, Avda U Antofagasta, Antofagasta 02800, Chile.
[Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, POB 11155-9161, Tehran, Iran.
[Rasmussen, R. Tronsgaard; Von Essen, C.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
[Skottfelt, J.] Open Univ, Dept Phys Sci, Ctr Elect Imaging, Milton Keynes MK7 6AA, Bucks, England.
[Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England.
[Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England.
[Surdej, J.; Wertz, O.] Inst Astrophys & Geophys, Allee 6 Aout 17,Bat B5c, B-4000 Liege, Belgium.
[Ulaczyk, K.] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England.
[Bryden, G.; Henderson, C. B.; Shvartzvald, Y.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Carey, S.] CALTECH, Spitzer, Ctr Sci, MS 220-6, Pasadena, CA 91109 USA.
[Abe, F.; Asakura, Y.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Nishioka, T.; Oyokawa, H.; Suzuki, D.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Private Bag 102-904, Auckland, New Zealand.
[Donachie, M.; Freeman, M.; Li, M. C. A.; Rattenbury, N.; Sharan, A.] Univ Auckland, Dept Phys, Private Bag 92019, Auckland, New Zealand.
[Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, 3037-5 Honjo, Okayama 7190232, Japan.
[Hirao, Y.; Koshimoto, N.; Nagakane, M.; Sumi, T.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Inayama, K.; Yonehara, A.] Kyoto Sangyo Univ, Dept Phys, Fac Sci, Kyoto 6038555, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, To] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan.
[Sullivan, D. J.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand.
[Tristram, J.] Mt John Univ Observ, POB 56, Lake Tekapo 8770, New Zealand.
[Han, C.; Choi, J-Y.; Park, H.; Jung, Y. K.; Shin, I-G.] Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea.
[Kerins, E.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England.
RP Street, RA (reprint author), LCOGT, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
RI Korhonen, Heidi/E-3065-2016; D'Ago, Giuseppe/N-8318-2016; Skowron,
Jan/M-5186-2014; Ranc, Clement/B-1958-2016;
OI Korhonen, Heidi/0000-0003-0529-1161; D'Ago,
Giuseppe/0000-0001-9697-7331; Skowron, Jan/0000-0002-2335-1730;
Tronsgaard, Rene/0000-0003-1001-0707; Ranc, Clement/0000-0003-2388-4534;
Dominik, Martin/0000-0002-3202-0343; Wang, Yi-Bo/0000-0002-5172-8558
FU National Science Centre, Poland grant MAESTRO [2014/14/A/ST9/00121]; JPL
[1500811]; NSF [AST 1516842, AST-1211875]; NASA; Creative Research
Initiative Program of National Research Foundation of Korea
[2009-0081561]; Regione Campania from POR-FSE Campania; JSPS; NASA
[NNX12AF54G]; NPRP from the Qatar National Research Fund (a member of
Qatar Foundation) [X019-1-006]; Chinese Academy of Sciences
[XDB09000000]; National Natural Science Foundation of China (NSFC)
[11333003, 11390372]; Villum Foundation; Communaut franaise de Belgique
Actions de recherche concertes Acadmie Wallonie-Europe; National Natural
Science Foundation of China [10873031, 11473066]; Gemini-Conicyt Fund
[32120036]; [JSPS23103002]; [JSPS24253004]; [JSPS26247023];
[JSPS25103508]; [23340064]
FX The OGLE project has received funding from the National Science Centre,
Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. Work by J.C.Y., A.G.,
and S.C. was supported by JPL grant 1500811. Work by W.Z. and A.G. was
supported by NSF AST 1516842.r Work by J.C.Y. was performed under
contract with the California Institute of Technology (Caltech)/Jet
Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship
Program executed by the NASA Exoplanet Science Institute. The Spitzer
Team thanks Christopher S. Kochanek for graciously trading us his
allocated observing time on the CTIO 1.3 m during the Spitzer campaign.r
Work by C.H. was supported by the Creative Research Initiative Program
(2009-0081561) of National Research Foundation of Korea.r G.D.
acknowledges Regione Campania for support from POR-FSE Campania
2014-2020.r T.S. acknowledges the financial support from the JSPS,
JSPS23103002,. JSPS24253004, and JSPS26247023. The MOA project is
supported by the grants JSPS25103508 and 23340064. The US portion of the
MOA Collaboration acknowledges financial support from the NSF
(AST-1211875) and NASA (NNX12AF54G).r Work by Y.S. was supported by an
appointment to the NASA Postdoctoral Program at the Jet Propulsion
Laboratory, administered by Oak Ridge Associated Universities through a
contract with NASA.r This publication was made possible by NPRP grant
#X019-1-006 from the Qatar National Research Fund (a member of Qatar
Foundation).r S.D. is supported by the Strategic Priority Research
Program "The Emergence of Cosmological Structures" of the Chinese
Academy of Sciences (grant No. XDB09000000).r Work by S.M. has been
supported by the Strategic Priority Research Program "The Emergence of
Cosmological Structures" of the Chinese Academy of Sciences Grant No.
XDB09000000, and by the National Natural Science Foundation of China
(NSFC) under grant numbers 11333003 and 11390372.r M.P.G.H. acknowledges
support from the Villum Foundation. Based on data collected by MiNDSTEp
with the Danish 1.54 m telescope at the ESO La Silla observatory. J..
Surdej and O.W. acknowledge support from the Communaut franaise de
Belgique Actions de recherche concertes Acadmie Wallonie-Europe. S.H.G.
and X.B.W. acknowledge the financial support from National Natural
Science Foundation of China through grants Nos. 10873031 and 11473066.r
N.P. acknowledges funding by the Gemini-Conicyt Fund, allocated to the
project No. 32120036.
NR 51
TC 12
Z9 12
U1 4
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 93
DI 10.3847/0004-637X/819/2/93
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700005
ER
PT J
AU Teodoro, M
Damineli, A
Heathcote, B
Richardson, ND
Moffat, AFJ
St-Jean, L
Russell, C
Gull, TR
Madura, TI
Pollard, K
Walter, F
Coimbra, A
Prates, R
Fernandez-Lajus, E
Gamen, RC
Hickel, G
Henrique, W
Navarete, F
Andrade, T
Jablonski, F
Luckas, P
Locke, M
Powles, J
Bohlseni, T
Chinii, R
Corcoran, MF
Hamaguchi, K
Groh, JH
Hillier, DJ
Weigelt, G
AF Teodoro, M.
Damineli, A.
Heathcote, B.
Richardson, N. D.
Moffat, A. F. J.
St-Jean, L.
Russell, C.
Gull, T. R.
Madura, T. I.
Pollard, K.
Walter, F.
Coimbra, A.
Prates, R.
Fernandez-Lajus, E.
Gamen, R. C.
Hickel, G.
Henrique, W.
Navarete, F.
Andrade, T.
Jablonski, F.
Luckas, P.
Locke, M.
Powles, J.
Bohlseni, T.
Chinii, R.
Corcoran, M. F.
Hamaguchi, K.
Groh, J. H.
Hillier, D. J.
Weigelt, G.
TI He II lambda 4686 EMISSION FROM THE MASSIVE BINARY SYSTEM IN eta CAR:
CONSTRAINTS TO THE ORBITAL ELEMENTS AND THE NATURE OF THE PERIODIC
MINIMA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; circumstellar matter; stars: individual (eta
Carinae); stars: massive
ID 3D RADIATIVE-TRANSFER; WIND-WIND COLLISION; 2014.6 SPECTROSCOPIC EVENT;
INNER COLLIDING WINDS; X-RAY MINIMUM; TRANSFER SIMULATIONS; IONIZATION
STRUCTURE; HOMUNCULUS NEBULA; LINE VARIABILITY; STELLAR WIND
AB Eta Carinae (eta Car) is an extremely massive binary system in which rapid spectrum variations occur near periastron. Most notably, near periastron the He II lambda 4686 line increases rapidly in strength, drops to a minimum value, then increases briefly before fading away. To understand this behavior, we conducted an intense spectroscopic monitoring of the He II lambda 4686 emission line across the 2014.6 periastron passage using ground-and space-based telescopes. Comparison with previous data confirmed the overall repeatability of the line equivalent width (EW), radial velocities, and the timing of the minimum, though the strongest peak was systematically larger in 2014 than in 2009 by 26%. The EW variations, combined with other measurements, yield an orbital period of 2022.7 +/- 0.3 days. The observed variability of the EW was reproduced by a model in which the line flux primarily arises at the apex of the wind-wind collision and scales inversely with the square of the stellar separation, if we account for the excess emission as the companion star plunges into the hot inner layers of the primary's atmosphere, and including absorption from the disturbed primary wind between the source and the observer. This model constrains the orbital inclination to 135 degrees-153 degrees, and the longitude of periastron to 234 degrees-252 degrees. It also suggests that periastron passage occurred on T-0 = 2456874.4 (+/- 1.3 days). Our model also reproduced EW variations from a polar view of the primary star as determined from the observed He II lambda 4686 emission scattered off the Homunculus nebula.
C1 [Teodoro, M.; Russell, C.; Gull, T. R.; Madura, T. I.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 667, Greenbelt, MD 20771 USA.
[Damineli, A.; Navarete, F.; Andrade, T.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, R Matao 1226,Cidade Univ, BR-05508900 Sao Paulo, Brazil.
[Heathcote, B.; Luckas, P.; Locke, M.; Powles, J.; Bohlseni, T.] SASER Team, 269 Domain Rd, South Yarra, Vic 3141, Australia.
[Richardson, N. D.; Moffat, A. F. J.; St-Jean, L.] Univ Montreal, Dept Phys, CP 6128,Succursale Ctr Ville, Montreal, PQ H3C 3J7, Canada.
[Pollard, K.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Walter, F.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Coimbra, A.; Prates, R.] Lab Nacl Astrof, R Estados Unidos 154, BR-37504364 Bairro Das Nacoes, Itajuba, Brazil.
[Fernandez-Lajus, E.; Gamen, R. C.] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, Paseo Bosque S-N,B1900FWA, RA-1900 La Plata, Buenos Aires, Argentina.
[Hickel, G.; Henrique, W.] Univ Fed Itajuba, Inst Fis & Quim, Ave BPS 1303, BR-37500062 Pinheirinho, Itajuba, Brazil.
[Jablonski, F.] Inst Nacl Pesquisas Espaciais, Div Astrofis, Ave Astronautas 1758, BR-12227010 Sao Jose Dos Campos, Brazil.
[Chinii, R.] Ruhr Univ Bochum, Astron Inst, Univ Str 150, D-44780 Bochum, Germany.
[Corcoran, M. F.; Hamaguchi, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Russell, C.; Hamaguchi, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Groh, J. H.] Observ Geneva, Chemin Maillettes 51, CH-1290 Versoix, Switzerland.
[Hillier, D. J.] Univ Pittsburgh, Dept Phys & Astron, 3941 OHara St, Pittsburgh, PA 15260 USA.
[Weigelt, G.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Teodoro, M.] Western Michigan Univ, Kalamazoo, MI 49008 USA.
[Richardson, N. D.] Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA.
[Madura, T. I.] Univ Space Res Assoc, 7178 Columbia Gateway Dr, Columbia, MD 20146 USA.
[Fernandez-Lajus, E.; Gamen, R. C.] Consejo Nacl Invest Cient & Tecn, Inst Astrofis La Plata, Paseo Bosque S-N,B1900FWA, La Plata, Buenos Aires, Argentina.
[Luckas, P.] Univ Western Australia, 35 Stirling Highway, Perth, WA 6009, Australia.
[Locke, M.] Canterbury Astron Soc, Canterbury, Kent, England.
[Chinii, R.] Univ Catolica Norte, Inst Astron, Ave Angamos 0610,Casilla 1280, Antofagasta, Chile.
[Hamaguchi, K.] Univ Maryland Baltimore Cty, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Hillier, D. J.] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr, 3941 OHara St, Pittsburgh, PA 15260 USA.
RP Teodoro, M (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 667, Greenbelt, MD 20771 USA.
EM mairan.teodoro@nasa.gov
RI Damineli, Augusto/P-8829-2016
OI Damineli, Augusto/0000-0002-7978-2994
FU CNPq/MCT-Brazil [201978/2012-1]; FAPESP [2011/51680-6]; office of the
Provost; NSERC (Canada); FRQNT (Quebec); CRAQ (Quebec); NASA; National
Aeronautics and Space Administration; [HST-GO 12508.02-A]
FX During part of this research, M.T. was supported by CNPq/MCT-Brazil
through grant 201978/2012-1. A.D. thanks FAPESP for financial support
through grant 2011/51680-6. F.W. thanks K. Davidson and R. Humphreys for
their discussions leading to part of these observations. Some of the
spectra were obtained under the aegis of Stony Brook University, whose
participation has been supported by the office of the Provost. We are
grateful to Pam Kilmartin and Fraser Gunn for helping with the
observations at MJUO. A.F.J.M. is grateful to financial aid to NSERC
(Canada) and FRQNT (Quebec). N.D. R. gratefully acknowledges his CRAQ
(Quebec) postdoctoral fellowship. D.J.H. acknowledges support from
HST-GO 12508.02-A. T.I.M. and C.M.P.R. are supported by an appointment
to the NASA Postdoctoral Program at the Goddard Space Flight Center,
administered by Oak Ridge Associated Universities through a contract
with NASA. We are grateful to STScI for support with the observational
schedule. This publication is based (in part) on spectroscopic data
obtained through the collaborative Southern Astro Spectroscopy Email
Ring (SASER) group.This research has made extensive use of NASA's
Astrophysics Data System, IDL Astronomy User's Library, and David
Fanning's IDL Coyote library. This research has made use of the NASA
Exoplanet Archive, which is operated by the California Institute of
Technology, under contract with the National Aeronautics and Space
Administration under the Exoplanet Exploration Program. We would like to
thank an anonymous referee for constructive suggestions that improved
the presentation of this work.
NR 85
TC 5
Z9 5
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2016
VL 819
IS 2
AR 131
DI 10.3847/0004-637X/819/2/131
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG8AV
UT WOS:000372305700043
ER
PT J
AU St Clair, JM
Rivera-Rios, JC
Crounse, JD
Knap, HC
Bates, KH
Teng, AP
Jorgensen, S
Kjaergaard, HG
Keutsch, FN
Wennberg, PO
AF St Clair, Jason M.
Rivera-Rios, Jean C.
Crounse, John D.
Knap, Hasse C.
Bates, Kelvin H.
Teng, Alex P.
Jorgensen, Solvejg
Kjaergaard, Henrik G.
Keutsch, Frank N.
Wennberg, Paul O.
TI Kinetics and Products of the Reaction of the First-Generation Isoprene
Hydroxy Hydroperoxide (ISOPOOH) with OH
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID SECONDARY ORGANIC AEROSOL; TROPOSPHERIC DEGRADATION; ATMOSPHERIC
CHEMISTRY; OXIDATION-PRODUCTS; EPOXIDE FORMATION; EPOXYDIOLS; NITRATES;
MODEL; PHOTOOXIDATION; MECHANISM
AB The atmospheric oxidation of isoprene by the OH radical leads to the formation of several isomers of an unsaturated hydroxy hydroperoxide, ISOPOOH. Oxidation of ISOPOOH by OH produces epoxydiols, IEPOX, which have been shown to contribute mass to secondary organic aerosol (SOA). We present kinetic rate constant measurements for OH + ISOPOOH using synthetic standards of the two major isomers: (1,2)- and (4,3)-ISOPOOH. At 297 K, the total,OH rate constant is 7.5 +/- 1.2 X 10(-11) cm(3) molecule(-1) s(-1) for (1,2)-ISOPOOH and 1.18 +/- 0.19 X 10(-13) cm(3) molecule(-1) s(-1) for (4,3)-ISOPOOH. Abstraction of the hydroperoxy hydrogen accounts for approximately 12% and 4% of the reactivity for (1,2)-ISOPOOH and (4,3)-ISOPOOH, respectively. The sum of all H-abstractions account for approximately 15% and 7% of the reactivity for (1,2)-ISOPOOH and (4,3)-ISOPOOH, respectively. The major product observed froth both ISOPOOH isomers was IEPOX (cis-beta and trans-beta isomers), with a similar to 2:1 preference for trans-beta IEPOX and similar total yields from each ISOPOOH isomer (similar to-70-80%). An IEPOX global production rate of more than 100 Tg C each year is estimated from this chemistry using a global 3D chemical transport model, similar to earlier estimates. Finally, following addition of OH to ISOPOOH, approximately 13% of the reactivity proceeds via addition of O-2 at 297 K and 745 Torr. In the presence of NO, these peroxy radicals lead to formation of small carbonyl compounds. Under HO2 dominated chemistry, no products are observed from these channels. We suggest that the major products, highly oxygenated organic peroxides, are lost to the chamber walls. In the atmosphere, formation of these compounds may contribute to organic aerosol mass.
C1 [St Clair, Jason M.; Crounse, John D.; Teng, Alex P.; Wennberg, Paul O.] CALTECH, Div Geol & Planetary Sci, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Bates, Kelvin H.] CALTECH, Div Chem & Chem Engn, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Wennberg, Paul O.] CALTECH, Div Engn & Appl Sci, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Rivera-Rios, Jean C.; Keutsch, Frank N.] Univ Wisconsin, Dept Chem, 1101 Univ Ave, Madison, WI 53706 USA.
[Keutsch, Frank N.] Harvard Univ, Paulson Sch Engn & Appl Sci, 12 Oxford St, Cambridge, MA 02138 USA.
[Keutsch, Frank N.] Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA.
[Knap, Hasse C.; Jorgensen, Solvejg] Univ Copenhagen, Dept Chem, DK-2100 Copenhagen O, Denmark.
[St Clair, Jason M.; Wennberg, Paul O.] NASA, Goddard Space Flight Ctr, UMBC JCET, Code 614, Greenbelt, MD 20771 USA.
RP St Clair, JM; Wennberg, PO (reprint author), NASA, Goddard Space Flight Ctr, UMBC JCET, Code 614, Greenbelt, MD 20771 USA.
EM jason.m.stclair@nasa.gov; wennberg@caltech.edu
RI Knap, Hasse/I-8798-2016; Jorgensen, Solvejg/A-1246-2011; Crounse,
John/C-3700-2014;
OI Knap, Hasse/0000-0002-8240-9496; Jorgensen, Solvejg/0000-0002-0255-1338;
Crounse, John/0000-0001-5443-729X; Teng, Alexander/0000-0002-6434-0501
FU National Science Foundation [AGS-1240604, AGS-1428482]; NASA
[NNX14AP46G-ACCDAM]; NSF [AGS 1247421, 1321987]; Danish Council for
Independent Research-Natural Sciences; Danish Center for Scientific
Computing
FX J.M.S.C., J.D.C., A.T., K.H.B., and P.O.W. thank the National Science
Foundation (AGS-1240604) and NASA (NNX14AP46G-ACCDAM) for supporting
this work. Development of the GC-ToF-CIMS is supported by an award from
the National Science Foundation's Major Research Instrumentation Program
(AGS-1428482). J.C.R. and F.N.K. acknowledge support from NSF Grant AGS
1247421 and 1321987. H.C.K, S.J., and H.G.K. thank the Danish Council
for Independent Research-Natural Sciences, and the Danish Center for
Scientific Computing for funding.
NR 46
TC 17
Z9 17
U1 45
U2 90
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD MAR 10
PY 2016
VL 120
IS 9
BP 1441
EP 1451
DI 10.1021/acs.jpca.5b06532
PG 11
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DG4KX
UT WOS:000372042200012
PM 26327174
ER
PT J
AU Ngeve, MN
Van der Stocken, T
Menemenlis, D
Koedam, N
Triest, L
AF Ngeve, Magdalene N.
Van der Stocken, Tom
Menemenlis, Dimitris
Koedam, Nico
Triest, Ludwig
TI Contrasting Effects of Historical Sea Level Rise and Contemporary Ocean
Currents on Regional Gene Flow of Rhizophora racemosa in Eastern
Atlantic Mangroves
SO PLOS ONE
LA English
DT Article
ID MICROSATELLITE NULL ALLELES; COLOMBIAN PACIFIC COAST; CLIMATE-CHANGE;
AVICENNIA-GERMINANS; POPULATION-STRUCTURE; MOZAMBIQUE CHANNEL;
EQUATORIAL-GUINEA; MUCRONATA LAM.; SEED DISPERSAL; CENTRAL-AFRICA
AB Mangroves are seafaring taxa through their hydrochorous propagules that have the potential to disperse over long distances. Therefore, investigating their patterns of gene flow provides insights on the processes involved in the spatial genetic structuring of populations. The coastline of Cameroon has a particular geomorphological history and coastal hydrology with complex contemporary patterns of ocean currents, which we hypothesize to have effects on the spatial configuration and composition of present-day mangroves within its spans. A total of 982 trees were sampled from 33 transects (11 sites) in 4 estuaries. Using 11 polymorphic SSR markers, we investigated genetic diversity and structure of Rhizophora racemosa, a widespread species in the region. Genetic diversity was low to moderate and genetic differentiation between nearly all population pairs was significant. Bayesian clustering analysis, PCoA, estimates of contemporary migration rates and identification of barriers to gene flow were used and complemented with estimated dispersal trajectories of hourly released virtual propagules, using high-resolution surface current from a mesoscale and tide-resolving ocean simulation. These indicate that the Cameroon Volcanic Line (CVL) is not a present-day barrier to gene flow. Rather, the Inter-Bioko-Cameroon (IBC) corridor, formed due to sea level rise, allows for connectivity between two mangrove areas that were isolated during glacial times by the CVL. Genetic data and numerical ocean simulations indicated that an oceanic convergence zone near the Cameroon Estuary complex (CEC) presents a strong barrier to gene flow, resulting in genetic discontinuities between the mangrove areas on either side. This convergence did not result in higher genetic diversity at the CEC as we had hypothesized. In conclusion, the genetic structure of Rhizophora racemosa is maintained by the contrasting effects of the contemporary oceanic convergence and historical climate change-induced sea level rise.
C1 [Ngeve, Magdalene N.; Van der Stocken, Tom; Koedam, Nico; Triest, Ludwig] Vrije Univ Brussel, Lab Plant Biol & Nat Management APNA, Dept Biol, Pleinlaan 2, B-1050 Brussels, Belgium.
[Menemenlis, Dimitris] CALTECH, Jet Prop Lab, Div Earth Sci, Pasadena, CA USA.
RP Ngeve, MN (reprint author), Vrije Univ Brussel, Lab Plant Biol & Nat Management APNA, Dept Biol, Pleinlaan 2, B-1050 Brussels, Belgium.
EM ngevem@yahoo.com
FU Vrije Universiteit Brussel-International Relations and Mobility Office
(VUB-IRMO) Doctoral Scholarship; Doctoral School NSE of the VUB
[NSE-TG-2013-82]; VUB; National Aeronautics and Space Administration
(NASA)
FX This study was financed by the Vrije Universiteit Brussel-International
Relations and Mobility Office (VUB-IRMO) Doctoral Scholarship awarded to
M.N. Ngeve. The Doctoral School NSE of the VUB also awarded a travel
grant (NSE-TG-2013-82) to M.N. Ngeve. The BAS 42 funding of the VUB also
supported the laboratory analyses of this study. The funders had no role
in study design, data collection and analysis, decision to publish, or
preparation of the manuscript.r We extend sincere gratitude to Ma
Christiana Nalova Ngenye, Mr. and Mrs. Ndoko Joseph (Ekondo-Titi), Pr.
and Mrs. Oben Samuel (Bekumu), Mr. Peter Elive Ikome (Douala), Pr. Eban
Daniel, Pr. Ntakim Clarence, Rev. Okala Dieudonne Bienvenue, Pr. and
Mrs. Atiko Pierre (Kribi), Elder Atkin Egbe Obie (Kribi), Eugene N.
Ngeve, and Ms Natalie Kana for logistical and field assistance. We are
also grateful to Tim Sierens for technical and laboratory assistance.
The numerical ocean modeling component of this research was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration
(NASA).
NR 116
TC 1
Z9 1
U1 11
U2 26
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD MAR 10
PY 2016
VL 11
IS 3
AR e0150950
DI 10.1371/journal.pone.0150950
PG 24
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DG3TL
UT WOS:000371993000085
PM 26964094
ER
PT J
AU Spiers, GD
Menzies, RT
Jacob, JC
AF Spiers, Gary D.
Menzies, Robert T.
Jacob, Joseph C.
TI Lidar reflectance from snow at 2.05 mu m wavelength as measured by the
JPL Airborne Laser Absorption Spectrometer
SO APPLIED OPTICS
LA English
DT Article
ID SURFACE WIND-SPEED; OPTICAL-PROPERTIES; HOT-SPOT; ATMOSPHERIC CO2;
BACKSCATTER; SPACE; SIGNATURES; WATER
AB We report airborne measurements of lidar directional reflectance (backscatter) from land surfaces at a wavelength in the 2.05 mu m CO2 absorption band, with emphasis on snow-covered surfaces in various natural environments. Lidar backscatter measurements using this instrument provide insight into the capabilities of lidar for both airborne and future global-scale CO2 measurements from low Earth orbit pertinent to the NASA Active Sensing of CO2 Emissions over Nights, Days, and Seasons mission. Lidar measurement capability is particularly useful when the use of solar scattering spectroscopy is not feasible for high-accuracy atmospheric CO2 measurements. Consequently, performance in high-latitude and winter season environments is an emphasis. Snowcovered surfaces are known to be dark in the CO2 band spectral regions. The quantitative backscatter data from these field measurements help to elucidate the range of backscatter values that can be expected in natural environments. (C) 2016 Optical Society of America
C1 [Spiers, Gary D.; Menzies, Robert T.; Jacob, Joseph C.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Menzies, RT (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM rmenzies@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX National Aeronautics and Space Administration.
NR 31
TC 0
Z9 0
U1 3
U2 7
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD MAR 10
PY 2016
VL 55
IS 8
BP 1978
EP 1986
DI 10.1364/AO.55.001978
PG 9
WC Optics
SC Optics
GA DG0TZ
UT WOS:000371779900026
PM 26974792
ER
PT J
AU Currie, T
Grady, CA
Cloutier, R
Konishi, M
Stassun, K
Debes, J
van der Marel, N
Muto, T
Jayawardhana, R
Ratzka, T
AF Currie, Thayne
Grady, Carol A.
Cloutier, Ryan
Konishi, Mihoko
Stassun, Keivan
Debes, John
van der Marel, Nienke
Muto, Takayuki
Jayawardhana, Ray
Ratzka, Thorsten
TI THE MATRYOSHKA DISK: KECK/NIRC2 DISCOVERY OF A SOLAR-SYSTEM-SCALE,
RADIALLY SEGREGATED RESIDUAL PROTOPLANETARY DISK AROUND HD 141569A
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planetary systems; stars: early-type; stars: individual (HD 141569A)
ID CIRCUMSTELLAR DISK; DEBRIS DISK; HR 8799; PLANET FORMATION; GIANT
PLANETS; EVOLUTION; SPECTROSCOPY; CONSTRAINTS; SUBTRACTION; ASYMMETRIES
AB Using Keck/NIRC2 L' (3.78 mu m) data, we report the direct imaging discovery of a scattered-light-resolved, solar-system-scale residual protoplanetary disk around the young A-type star HD 141569A, interior to and concentric with the two ring-like structures at wider separations. The disk is resolved down to similar to 0 ''.25 and appears as an arc-like rim with attached hook-like features. It is located at an angular separation intermediate between that of warm CO gas identified from spatially resolved mid-infrared spectroscopy and diffuse dust emission recently discovered with the Hubble Space Telescope. The inner disk has a radius of similar to 39 au, a position angle consistent with north. up, and. an inclination of i similar to 56 degrees. and has a center offset from the star. Forward. modeling of the disk favors a thick torus-like emission sharply truncated at separations beyond the torus's photocenter and heavily depleted at smaller separations. In particular, the best-fit density power law for the dust suggests that the inner disk dust and gas (as probed by CO) are radially segregated, a feature consistent with the dust trapping mechanism inferred from observations of "canonical" transitional disks. However, the inner disk component may instead be explained by radiation pressure-induced migration in optically thin conditions, in contrast to the two stellar companion/planet-influenced ring-like structures at wider separations. HD 141569A's circumstellar environment-with three nested, gapped, concentric dust populations-is an excellent laboratory for understanding the relationship between planet formation and the evolution of both dust grains and disk architecture.
C1 [Currie, Thayne] Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA.
[Grady, Carol A.] NASA Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD USA.
[Cloutier, Ryan] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
[Konishi, Mihoko] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Osaka, Japan.
[Stassun, Keivan] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Debes, John] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[van der Marel, Nienke] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Muto, Takayuki] Kogakuin Univ, Tokyo, Japan.
[Jayawardhana, Ray] York Univ, Dept Phys & Astron, Toronto, ON M3J 2R7, Canada.
[Ratzka, Thorsten] Graz Univ, NAWI Graz, Inst Phys IGAM, Graz, Austria.
RP Currie, T (reprint author), Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA.
OI Ratzka, Thorsten/0000-0001-9557-8232
FU NASA Origins of Solar Systems program [NNG13PB64P]
FX We thank Scott Kenyon and Mengshu Xu for helpful comments. C.A.G. is
supported under the NASA Origins of Solar Systems program NNG13PB64P. We
wish to emphasize the pivotal cultural role and reverence that the
summit of Maunakea has always had within the indigenous Hawaiian
community. We are most fortunate to have the privilege to conduct
scientific observations from this mountain.
NR 45
TC 2
Z9 2
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2016
VL 819
IS 2
AR L26
DI 10.3847/2041-8205/819/2/L26
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG0XC
UT WOS:000371788300010
ER
PT J
AU King, AL
Tomsick, JA
Miller, JM
Chenevez, J
Barret, D
Boggs, SE
Chakrabarty, D
Christensen, FE
Craig, WW
Furst, F
Hailey, CJ
Harrison, FA
Parker, ML
Stern, D
Romano, P
Walton, DJ
Zhang, WW
AF King, Ashley L.
Tomsick, John A.
Miller, Jon M.
Chenevez, Jerome
Barret, Didier
Boggs, Steven E.
Chakrabarty, Deepto
Christensen, Finn E.
Craig, William W.
Fuerst, Felix
Hailey, Charles J.
Harrison, Fiona A.
Parker, Michael L.
Stern, Daniel
Romano, Patrizia
Walton, Dominic J.
Zhang, William W.
TI MEASURING A TRUNCATED DISK IN AQUILA X-1
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; magnetic fields; stars: neutron; X-rays:
binaries; X-rays: bursts
ID X-RAY BINARIES; ACCRETING MILLISECOND PULSAR; BLACK-HOLE CANDIDATES; AQL
X-1; NEUTRON-STARS; 4U 1705-44; MAGNETIC-FIELD; LIGHT CURVES; SOFT
STATES; XMM-NEWTON
AB We present NuSTAR and Swift observations of the neutron star Aquila X-1 during the peak of its 2014 July outburst. The spectrum is soft with strong evidence for a broad Fe Ka line. Modeled with a relativistically broadened reflection model, we find that the inner disk is truncated with an inner radius of 15 +/- 3R(G). The disk is likely truncated by either the boundary layer and/or a magnetic field. Associating the truncated inner disk with pressure from a magnetic field gives an upper limit of B < 5 +/- 2 x 10(8) G. Although the radius is truncated far from the stellar surface, material is still reaching the neutron star surface as evidenced by the X-ray burst present in the NuSTAR observation.
C1 [King, Ashley L.] Stanford Univ, KIPAC, 452 Lomita Mall, Stanford, CA 94305 USA.
[Tomsick, John A.; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
[Miller, Jon M.] Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA.
[Chenevez, Jerome] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327-328, DK-2800 Lyngby, Denmark.
[Barret, Didier] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Barret, Didier] CNRS, IRAP, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France.
[Chakrabarty, Deepto] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Fuerst, Felix; Harrison, Fiona A.; Walton, Dominic J.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[Parker, Michael L.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Stern, Daniel; Walton, Dominic J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Romano, Patrizia] INAF IASF Palermo, Via Ugo La Malfa 153, I-90146 Palermo, Italy.
[Zhang, William W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP King, AL (reprint author), Stanford Univ, KIPAC, 452 Lomita Mall, Stanford, CA 94305 USA.
EM ashking@stanford.edu
RI Boggs, Steven/E-4170-2015
OI Boggs, Steven/0000-0001-9567-4224
FU NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center
[PF4-150125]; NASA [NAS8-03060]; ASI-INAF [I/037/12/0, I/004/11/0];
ESA/PRODEX [90057]; National Aeronautics and Space Administration
FX The authors thank the referee for their invaluable comments. A.L.K.
would like to thank the support for this work, which was provided by
NASA through Einstein Postdoctoral Fellowship grant number PF4-150125
awarded by the Chandra X-ray Center, operated by the Smithsonian
Astrophysical Observatory for NASA under contract NAS8-03060. P.R.
acknowledges financial contribution from contract ASI-INAF I/004/11/0
and ASI-INAF I/037/12/0. J.C. is grateful for financial support from
ESA/PRODEX No. 90057. This work made use of data from the NuSTAR
mission, a project led by the California Institute of Technology,
managed by the Jet Propulsion Laboratory, and funded by the National
Aeronautics and Space Administration. This research has made use of the
NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI
Science Data Center (ASDC, Italy) and the California Institute of
Technology (USA).
NR 48
TC 4
Z9 4
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2016
VL 819
IS 2
AR L29
DI 10.3847/2041-8205/819/2/L29
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG0XC
UT WOS:000371788300013
ER
PT J
AU Penn, M
Krucker, S
Hudson, H
Jhabvala, M
Jennings, D
Lunsford, A
Kaufmann, P
AF Penn, Matt
Krucker, Saem
Hudson, Hugh
Jhabvala, Murzy
Jennings, Don
Lunsford, Allen
Kaufmann, Pierre
TI SPECTRAL AND IMAGING OBSERVATIONS OF A WHITE-LIGHT SOLAR FLARE IN THE
MID-INFRARED
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: flares; Sun: infrared
ID CONTINUUM; MICRONS; RHESSI; MODELS
AB We report high-resolution observations at mid-infrared wavelengths of a minor solar flare, SOL2014-09-24T17:50 (C7.0), using Quantum Well Infrared Photodetector cameras at an auxiliary of the McMath-Pierce telescope. The flare emissions, the first simultaneous observations in two mid-infrared bands at 5.2 and 8.2 mu m with white-light and hard X-ray coverage, revealed impulsive time variability with increases on timescales of similar to 4 s followed by exponential decay at similar to 10 s in two bright regions separated by about 13 ''. The brightest source is compact, unresolved spatially at the diffraction limit (1 ''.72 at 5.2 mu m). We identify the IR sources as flare ribbons also seen in white-light emission at 6173 angstrom. observed by SDO/HMI, with twin hard X-ray sources observed by Reuven Ramaty High Energy Solar Spectroscopic Imager, and with EUV sources (e.g., 94 angstrom) observed by SDO/AIA. The two infrared points have nearly the same flux density (f(nu), Wm(-2) Hz) and extrapolate to a level of about an order of magnitude below that observed in the visible band by HMI, but with a flux of more than two orders of magnitude above the free-free continuum from the hot (similar to 15 MK) coronal flare loop observed in the X-ray range. The observations suggest that the IR emission is optically thin; this constraint and others suggest major contributions from a density less than about 4 x 10(13) cm(-3). We tentatively interpret this emission mechanism as predominantly free-free emission in a highly ionized but cool and rather dense chromospheric region.
C1 [Penn, Matt] Natl Solar Observ, Tucson, AZ 85719 USA.
[Krucker, Saem] Univ Appl Sci & Arts Northwestern Switzerland, CH-5210 Windisch, Switzerland.
[Krucker, Saem; Hudson, Hugh] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Jhabvala, Murzy] NASA Goddard Space Flight Ctr, Instrument Syst & Technol Div, Code 550, Greenbelt, MD USA.
[Jennings, Don] NASA Goddard Space Flight Ctr, Detector Syst Branch, Code 553, Greenbelt, MD USA.
[Lunsford, Allen] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Kaufmann, Pierre] Univ Prebiteriana Mackenzie, Sch Engn, Ctr Radio Astron & Astrophys, Sao Paulo, Brazil.
RP Penn, M (reprint author), Natl Solar Observ, Tucson, AZ 85719 USA.
EM mpenn@nso.edu
OI Hudson, Hugh/0000-0001-5685-1283
FU NASA Small Business Innovative Research (SBIR) program; Goddard Space
Flight Center; QmagiQ, LLC (Nashua, NH); Swiss National Science
Foundation [200021-140308]; NASA [NAS 5-98033, NNX11AP05]
FX The development of the QWIP cameras was supported by the NASA Small
Business Innovative Research (SBIR) program, in collaboration with the
Goddard Space Flight Center and QmagiQ, LLC (Nashua, NH). S.K. is
supported by Swiss National Science Foundation (200021-140308) and
through NASA contract NAS 5-98033 for RHESSI. H.S.H. thanks NASA for
support under contract NNX11AP05. The authors thank Paulo Simoes for
correcting errors in the original draft, and Lucia Kleint for detailed
comments on the preprint.
NR 21
TC 1
Z9 1
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAR 10
PY 2016
VL 819
IS 2
AR L30
DI 10.3847/2041-8205/819/2/L30
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DG0XC
UT WOS:000371788300014
ER
PT J
AU Ortiz, N
Mangel, JC
Wang, J
Alfaro-Shigueto, J
Pingo, S
Jimenez, A
Suarez, T
Swimmer, Y
Carvalho, F
Godley, BJ
AF Ortiz, Natalia
Mangel, Jeffrey C.
Wang, John
Alfaro-Shigueto, Joanna
Pingo, Sergio
Jimenez, Astrid
Suarez, Tania
Swimmer, Yonat
Carvalho, Felipe
Godley, Brendan J.
TI Reducing green turtle bycatch in small-scale fisheries using illuminated
gillnets: the cost of saving a sea turtle
SO MARINE ECOLOGY PROGRESS SERIES
LA English
DT Article
DE LEDs; Green turtles; CPUE; Small-scale fishery; Bycatch; Peru
ID MARINE PROTECTED AREAS; LONGLINE FISHERIES; BY-CATCH; PELAGIC LONGLINES;
LOGGERHEAD TURTLE; EXCLUDER DEVICES; SEABIRD BYCATCH; GLOBAL PATTERNS;
NET FISHERIES; CIRCLE HOOKS
AB Gillnet fisheries exist throughout the oceans and have been implicated in high by catch rates of sea turtles. In this study, we examined the effectiveness of illuminating nets with light-emitting diodes (LEDs) placed on floatlines in order to reduce sea turtle bycatch in a small-scale bottom-set gillnet fishery. In Sechura Bay, northern Peru, 114 pairs of control and illuminated nets were deployed. The predicted mean catch per unit effort (CPUE) of target species, standardized for environmental variables using generalized additive model (GAM) analysis, was similar for both control and illuminated nets. In contrast, the predicted mean CPUE of green turtles Chelonia mydas was reduced by 63.9% in illuminated nets. A total of 125 green turtles were caught in control nets, while 62 were caught in illuminated nets. This statistically significant re duction (GAM analysis, p < 0.05) in sea turtle bycatch suggests that net illumination could be an effective conservation tool. Challenges to implementing the use of LEDs include equipment costs, increased net handling times, and limited awareness among fishermen regarding the effectiveness of this technology. Cost estimates for preventing a single sea turtle catch are as low as 34 USD, while the costs to outfit the entire gillnet fishery in Sechura Bay can be as low as 9200 USD. Understanding these cost challenges emphasizes the need for institutional support from national ministries, inter national non-governmental organizations and the broader fisheries industry to make possible widespread implementation of net illumination as a sea turtle bycatch reduction strategy.
C1 [Ortiz, Natalia; Mangel, Jeffrey C.; Alfaro-Shigueto, Joanna; Pingo, Sergio; Jimenez, Astrid; Suarez, Tania] ProDelphinus, Octavio Bernal 572-5, Lima 11, Peru.
[Mangel, Jeffrey C.; Alfaro-Shigueto, Joanna; Godley, Brendan J.] Univ Exeter, Ctr Ecol & Conservat, Penryn TR10 9EZ, Cornwall, England.
[Wang, John; Swimmer, Yonat; Carvalho, Felipe] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA.
[Alfaro-Shigueto, Joanna] Univ Cient Sur, Fac Biol Marina, Panamer Km 19, Lima, Peru.
[Carvalho, Felipe] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI USA.
RP Mangel, JC (reprint author), ProDelphinus, Octavio Bernal 572-5, Lima 11, Peru.; Mangel, JC (reprint author), Univ Exeter, Ctr Ecol & Conservat, Penryn TR10 9EZ, Cornwall, England.
EM j.mangel@exeter.ac.uk
FU ProDelphinus; Darwin Initiative; National Marine Fisheries Service of
the National Oceanic and Atmospheric Administration; University of
Hawaii Joint Institute for Marine and Atmospheric Research
FX We thank the following field assistants who participated in data
collection: E. Alfaro, N. Balducci, E. Campbell, T. Clay, P. Doherty, A.
Luna, H. Parra, A. Pasara, and A. Ugolini. We also thank the fishermen
and their families at Constante, Piura, Peru, for their support on every
fishing trip. This work and study was supported by ProDelphinus, the
Darwin Initiative, the National Marine Fisheries Service of the National
Oceanic and Atmospheric Administration, and the University of Hawaii
Joint Institute for Marine and Atmospheric Research.
NR 60
TC 2
Z9 2
U1 19
U2 35
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 0171-8630
EI 1616-1599
J9 MAR ECOL PROG SER
JI Mar. Ecol.-Prog. Ser.
PD MAR 8
PY 2016
VL 545
BP 251
EP 259
DI 10.3354/meps11610
PG 9
WC Ecology; Marine & Freshwater Biology; Oceanography
SC Environmental Sciences & Ecology; Marine & Freshwater Biology;
Oceanography
GA DH1UZ
UT WOS:000372571700020
ER
PT J
AU Nguyen, BN
Cudjoe, E
Douglas, A
Scheiman, D
McCorkle, L
Meador, MAB
Rowan, SJ
AF Nguyen, Baochau N.
Cudjoe, Elvis
Douglas, Anna
Scheiman, Daniel
McCorkle, Linda
Meador, Mary Ann B.
Rowan, Stuart J.
TI Polyimide Cellulose Nanocrystal Composite Aerogels
SO MACROMOLECULES
LA English
DT Article
ID AMINE-MODIFIED SILICA; SYNDIOTACTIC POLYSTYRENE AEROGELS; POLYMER
NANOCOMPOSITES; MECHANICALLY STRONG; ORGANIC AEROGELS; MONOLITHIC
AEROGELS; THERMAL INSULATION; CARBON AEROGELS; FORMALDEHYDE; NANOFIBERS
AB Cellulose nanocrystals derived from tunicates (t-CNC) were used as a reinforcing nanofiller for polyimide aerogels. Two sets of polyimide aerogels, containing either 2,2'-dimethylbenzidine (DMBZ) or 4,4'-oxydianiline (ODA) and 3,3',4,4'-biphenyltetracarboxylic acid dianhydride (BPDA) cross-linked with 1,3,5-tris (4-aminophenoxy)benzene (TAB), were studied. Total solids composition of the aerogels were kept constant at 7.5 wt %, with 0-13.33 wt % of the total solids being the carboxylic acid-functionalized t-CNC (t-CNC-COOH) filler. The incorporation of the t-CNC-COOH, with carboxylic acid content of either 560 or 920 mmol/kg, in the polyimide aerogel networks improved both physical and mechanical properties of the final materials. Isothermal aging of t-CNC-COOH aerogel composites was also conducted at 150 and 200 degrees C for 24 h. Higher content t-CNC-COOH/polyimide aerogels showed less change in their density and reduced shrinkage during aging, which further emphasized the effect of the t-CNC-COOH reinforcement in retaining the structural integrity of the aerogel.
C1 [Nguyen, Baochau N.; Scheiman, Daniel; McCorkle, Linda] Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.
[Douglas, Anna; Meador, Mary Ann B.] NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
[Cudjoe, Elvis; Rowan, Stuart J.] Case Western Reserve Univ, Dept Macromol Sci & Engn, 2100 Adelbert Rd, Cleveland, OH 44106 USA.
RP Meador, MAB (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.; Rowan, SJ (reprint author), Case Western Reserve Univ, Dept Macromol Sci & Engn, 2100 Adelbert Rd, Cleveland, OH 44106 USA.
EM maryann.meador@nasa.gov; stuart.rowan@case.edu
OI Meador, Mary Ann/0000-0003-2513-7372
FU NASA Space Technology Mission Directorate Center Innovation Fund;
[NSF-DMR-1204948]
FX We thank the NASA Space Technology Mission Directorate Center Innovation
Fund and the NSF-DMR-1204948 for support of the project. We also thank
Dr. Haiquan Guo for nitrogen sorption experiments, Dan Haas for
assistance with supercritical drying, and Brian Michal for delivering
samples to and from CWRU and NASA.
NR 63
TC 5
Z9 5
U1 50
U2 162
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0024-9297
EI 1520-5835
J9 MACROMOLECULES
JI Macromolecules
PD MAR 8
PY 2016
VL 49
IS 5
BP 1692
EP 1703
DI 10.1021/acs.macromol.5b01573
PG 12
WC Polymer Science
SC Polymer Science
GA DG1TT
UT WOS:000371851100021
ER
PT J
AU Aramaki, T
Boggs, S
Bufalino, S
Dal, L
von Doetinchem, P
Donato, F
Fornengo, N
Fuke, H
Grefe, M
Hailey, C
Hamilton, B
Ibarra, A
Mitchell, J
Mognet, I
Ong, RA
Pereira, R
Perez, K
Putze, A
Raklev, A
Salati, P
Sasaki, M
Tarle, G
Urbano, A
Vittino, A
Wild, S
Xue, W
Yoshimura, K
AF Aramaki, T.
Boggs, S.
Bufalino, S.
Dal, L.
von Doetinchem, P.
Donato, F.
Fornengo, N.
Fuke, H.
Grefe, M.
Hailey, C.
Hamilton, B.
Ibarra, A.
Mitchell, J.
Mognet, I.
Ong, R. A.
Pereira, R.
Perez, K.
Putze, A.
Raklev, A.
Salati, P.
Sasaki, M.
Tarle, G.
Urbano, A.
Vittino, A.
Wild, S.
Xue, W.
Yoshimura, K.
TI Review of the theoretical and experimental status of dark matter
identification with cosmic-ray antideuterons
SO PHYSICS REPORTS-REVIEW SECTION OF PHYSICS LETTERS
LA English
DT Review
DE Antideuteron; Cosmic ray; Dark matter; Coalescence; Propagation
ID INTERNATIONAL-SPACE-STATION; ENERGY PROTON-BOMBARDMENT; ALPHA MAGNETIC
SPECTROMETER; PRIMORDIAL BLACK-HOLES; DISTANT SC-1 GALAXIES; VELOCITY
ANISOTROPY; INTERSTELLAR-MEDIUM; PARTICLE PHYSICS; PGAPS EXPERIMENT;
DIFFUSION-MODEL
AB Recent years have seen increased theoretical and experimental effort towards the first ever detection of cosmic-ray antideuterons, in particular as an indirect signature of dark matter annihilation or decay. In contrast to indirect dark matter searches using positrons, antiprotons, or gamma-rays, which suffer from relatively high and uncertain astrophysical backgrounds, searches with antideuterons benefit from very suppressed conventional backgrounds, offering a potential breakthrough in unexplored phase space for dark matter. This article is based on the first dedicated cosmic-ray antideuteron workshop, which was held at UCLA in June 2014. It reviews broad classes of dark matter candidates that result in detectable cosmic-ray antideuteron fluxes, as well as the status and prospects of cur rent experimental searches. The coalescence model of antideuteron production and the influence of antideuteron measurements at particle colliders are discussed. This is followed by a review of the modeling of antideuteron propagation through the magnetic fields, plasma currents, and molecular material of our Galaxy, the solar system, the Earth's geomagnetic field, and the atmosphere. Finally, the three ongoing or planned experiments that are sensitive to cosmic-ray antideuterons, BESS, AMS-02, and GAPS, are detailed. As cosmic-ray antideuteron detection is a rare event search, multiple experiments with orthogonal techniques and backgrounds are essential. Therefore, the combination of AMS-02 and GAPS antideuteron searches is highly desirable. Many theoretical and experimental groups have contributed to these studies over the last decade, this review aims to provide the first coherent discussion of the relevant dark matter theories that antideuterons probe, the challenges to predictions and interpretations of antideuteron signals, and the experimental efforts toward cosmic antideuteron detection. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Aramaki, T.; Hailey, C.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[Aramaki, T.] SLAC Natl Accelerator Lab, Menlo Pk, CA USA.
[Boggs, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94709 USA.
[Bufalino, S.; Donato, F.; Fornengo, N.; Vittino, A.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Dal, L.; Raklev, A.] Univ Oslo, Dept Phys, POB 1048, N-0316 Oslo, Norway.
[von Doetinchem, P.; Pereira, R.] Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Donato, F.; Fornengo, N.; Vittino, A.] Univ Turin, Dept Phys, I-10125 Turin, Italy.
[Fuke, H.] Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Grefe, M.] Univ Hamburg, Inst Theoret Phys 2, D-22761 Hamburg, Germany.
[Hamilton, B.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Ibarra, A.; Wild, S.] Tech Univ Munich, Phys Dept T30D, D-85748 Garching, Germany.
[Mitchell, J.; Sasaki, M.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
[Mognet, I.; Ong, R. A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Perez, K.] Haverford Coll, Haverford, PA 19041 USA.
[Putze, A.; Salati, P.] Univ Savoie Mt Blanc, CNRS, LAPTh, F-74941 Annecy Le Vieux, France.
[Putze, A.] Univ Savoie Mt Blanc, CNRS, LAPP, IN2P3, F-74941 Annecy Le Vieux, France.
[Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Urbano, A.] SISSA Int Sch Adv Studies, I-34136 Trieste, Italy.
[Xue, W.] MIT, Ctr Theoret Phys, Cambridge, MA 02139 USA.
[Yoshimura, K.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan.
RP von Doetinchem, P (reprint author), Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA.
EM philipvd@hawaii.edu
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Grefe, Michael/0000-0003-1346-5133
FU University of California, Los Angeles; Forschungs- und
Wissenschaftsstiftung Hamburg through the program "Astroparticle Physics
with Multiple Messengers"; Marie Curie ITN "INVISIBLES"
[PITN-GA-2011-289442]; DFG cluster of excellence "Origin and Structure
of the Universe"; National Science Foundation [1202958]; Studienstiftung
des Deutschen Volkes [2008 0315]; TUM Graduate School
FX The first dedicated cosmic-ray antideuteron workshop at UCLA in June
2014 was supported, in part, by the University of California, Los
Angeles. The organizers of the workshop, PvD and RO, would like to thank
all participants for a successful and fruitful meeting. The work of MG
was supported by the Forschungs- und Wissenschaftsstiftung Hamburg
through the program "Astroparticle Physics with Multiple Messengers" and
by the Marie Curie ITN "INVISIBLES" under grant number
PITN-GA-2011-289442. The work of AI was partially supported by the DFG
cluster of excellence "Origin and Structure of the Universe". KPs work
was supported in part by the National Science Foundation under Award No.
1202958. SW was supported by the Studienstiftung des Deutschen Volkes
(No. 2008 0315) and by the TUM Graduate School.
NR 215
TC 1
Z9 1
U1 2
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0370-1573
EI 1873-6270
J9 PHYS REP
JI Phys. Rep.-Rev. Sec. Phys. Lett.
PD MAR 7
PY 2016
VL 618
BP 1
EP 37
DI 10.1016/j.physrep.2016.01.002
PG 37
WC Physics, Multidisciplinary
SC Physics
GA DH1QG
UT WOS:000372559400001
ER
PT J
AU Matthia, D
Ehresmann, B
Lohf, H
Kohler, J
Zeitlin, C
Appel, J
Sato, T
Slaba, T
Martin, C
Berger, T
Boehm, E
Boettcher, S
Brinza, DE
Burmeister, S
Guo, J
Hassler, DM
Posner, A
Rafkin, SCR
Reitz, G
Wilson, JW
Wimmer-Schweingruber, RF
AF Matthia, Daniel
Ehresmann, Bent
Lohf, Henning
Koehler, Jan
Zeitlin, Cary
Appel, Jan
Sato, Tatsuhiko
Slaba, Tony
Martin, Cesar
Berger, Thomas
Boehm, Eckart
Boettcher, Stephan
Brinza, David E.
Burmeister, Soenke
Guo, Jingnan
Hassler, Donald M.
Posner, Arik
Rafkin, Scot C. R.
Reitz, Guenther
Wilson, John W.
Wimmer-Schweingruber, Robert F.
TI The Martian surface radiation environment - a comparison of models and
MSL/RAD measurements
SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE
LA English
DT Article
DE Mars; Galactic cosmic radiation; Radiation environment; Human
exploration; Numerical models; Exposure
ID ENERGETIC PARTICLE RADIATION; COSMIC-RAY MODEL; GENERAL-CIRCULATION;
ASSESSMENT DETECTOR; IONIZING-RADIATION; MARS; HZETRN; SCIENCE;
SIMULATION; DYNAMICS
AB Context: The Radiation Assessment Detector (RAD) on the Mars Science Laboratory (MSL) has been measuring the radiation environment on the surface of Mars since August 6th 2012. MSL-RAD is the first instrument to provide detailed information about charged and neutral particle spectra and dose rates on the Martian surface, and one of the primary objectives of the RAD investigation is to help improve and validate current radiation transport models.
Aims: Applying different numerical transport models with boundary conditions derived from the MSL-RAD environment the goal of this work was to both provide predictions for the particle spectra and the radiation exposure on the Martian surface complementing the RAD sensitive range and, at the same time, validate the results with the experimental data, where applicable. Such validated models can be used to predict dose rates for future manned missions as well as for performing shield optimization studies.
Methods: Several particle transport models (GEANT4, PHITS, HZETRN/OLTARIS) were used to predict the particle flux and the corresponding radiation environment caused by galactic cosmic radiation on Mars. From the calculated particle spectra the dose rates on the surface are estimated.
Results: Calculations of particle spectra and dose rates induced by galactic cosmic radiation on the Martian surface are presented. Although good agreement is found in many cases for the different transport codes, GEANT4, PHITS, and HZETRN/OLTARIS, some models still show large, sometimes order of magnitude discrepancies in certain particle spectra. We have found that RAD data is helping to make better choices of input parameters and physical models. Elements of these validated models can be applied to more detailed studies on how the radiation environment is influenced by solar modulation, Martian atmosphere and soil, and changes due to the Martian seasonal pressure cycle. By extending the range of the calculated particle spectra with respect to the experimental data additional information about the radiation environment is gained, and the contribution of different particle species to the dose is estimated.
C1 [Matthia, Daniel; Berger, Thomas; Reitz, Guenther] German Aerosp Ctr, Inst Aerosp Med, D-51147 Cologne, Germany.
[Ehresmann, Bent; Hassler, Donald M.; Rafkin, Scot C. R.] Southwest Res Inst, Space Sci & Engn Div, Boulder, CO 80302 USA.
[Lohf, Henning; Koehler, Jan; Appel, Jan; Martin, Cesar; Boehm, Eckart; Boettcher, Stephan; Burmeister, Soenke; Guo, Jingnan; Wimmer-Schweingruber, Robert F.] Univ Kiel, Inst Expt & Appl Phys, Olshaussenstr 40, D-24118 Kiel, Germany.
[Zeitlin, Cary] Southwest Res Inst, Space Sci & Engn Div, Durham, NH 03824 USA.
[Sato, Tatsuhiko] Japan Atom Energy Agcy, Tokai, Ibaraki 3191195, Japan.
[Slaba, Tony] NASA, Langley Res Ctr, 2 West Reid St,MS 188E, Hampton, VA 23681 USA.
[Brinza, David E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Posner, Arik] NASA Headquarters, Washington, DC 20546 USA.
[Wilson, John W.] Old Dominion Univ, Norfolk, VA 23529 USA.
RP Matthia, D (reprint author), German Aerosp Ctr, Inst Aerosp Med, D-51147 Cologne, Germany.
EM Daniel.Matthiae@dlr.de
OI Matthia, Daniel/0000-0003-1507-0143; Berger, Thomas/0000-0003-3319-5740
FU NASA (HEOMD) under JPL Subcontract [1273039]; DLR's Space Administration
Grants [50QM0501, 50QM1201]; DLR
FX RAD is supported by NASA (HEOMD) under JPL Subcontract 1273039 to
Southwest Research Institute and in Germany by DLR and DLR's Space
Administration Grants 50QM0501 and 50QM1201 to the Christian Albrechts
University, Kiel. Part of this research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 68
TC 4
Z9 4
U1 5
U2 11
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 2115-7251
J9 J SPACE WEATHER SPAC
JI J. Space Weather Space Clim.
PD MAR 4
PY 2016
VL 6
AR A13
DI 10.1051/swsc/2016008
PG 17
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA DM9NG
UT WOS:000376692400001
ER
PT J
AU Ueland, M
Blanes, L
Taudte, RV
Stuart, BH
Cole, N
Willis, P
Roux, C
Doble, P
AF Ueland, Maiken
Blanes, Lucas
Taudte, Regina V.
Stuart, Barbara H.
Cole, Nerida
Willis, Peter
Roux, Claude
Doble, Philip
TI Capillary-driven microfluidic paper-based analytical devices for lab on
a chip screening of explosive residues in soil
SO JOURNAL OF CHROMATOGRAPHY A
LA English
DT Article
DE Explosive detection; Lab on a chip; mu PADs
ID NITROAROMATIC EXPLOSIVES; LIQUID CHROMATOGRAPHY; DEGRADATION-PRODUCTS;
ELECTROPHORESIS; EXTRACTION; MICROCHIP; IDENTIFICATION; SEPARATION;
SAMPLES
AB A novel microfluidic paper-based analytical device (mu PAD) was designed to filter, extract, and pre-concentrate explosives from soil for direct analysis by a lab on a chip (LOC) device. The explosives were extracted via immersion of wax-printed mu PADs directly into methanol soil suspensions for 10 min, whereby dissolved explosives travelled upwards into the mu PAD circular sampling reservoir. A chad was punched from the sampling reservoir and inserted into a LOC well containing the separation buffer for direct analysis, avoiding any further extraction step. Eight target explosives were separated and identified by fluorescence quenching. The minimum detectable amounts for all eight explosives were between 1.4 and 5.6 ng with recoveries ranging from 53-82% from the paper chad, and 12-40% from soil. This method provides a robust and simple extraction method for rapid identification of explosives in complex soil samples. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Ueland, Maiken; Blanes, Lucas; Taudte, Regina V.; Stuart, Barbara H.; Cole, Nerida; Roux, Claude; Doble, Philip] Univ Technol Sydney, Ctr Forens Sci, Broadway, NSW 2007, Australia.
[Willis, Peter] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Doble, P (reprint author), Univ Technol Sydney, Sch Chem & Forens Sci, Analyt Chem, POB 123, Broadway, NSW 2007, Australia.; Doble, P (reprint author), Univ Technol Sydney, Sch Chem & Forens Sci, Elemental Bioimaging Facil, POB 123, Broadway, NSW 2007, Australia.
EM Maiken.Ueland@student.uts.edu.au; Lucas.Blanes@uts.edu.au;
Regina.Taudte@uts.edu.au; Barbara.Stuart-1@uts.edu.au;
nerida.cole@uts.edu.au; Peter.A.Willis@jpl.nasa.gov;
Claude.Roux@uts.edu.au; Philip.Doble@uts.edu.au
RI Roux, Claude/I-8052-2014; Willis, Peter/I-6621-2012;
OI Roux, Claude/0000-0003-3610-420X; Doble, Philip/0000-0002-8472-1301;
Stuart, Barbara/0000-0001-9540-4435
FU Australian Research Council Linkage Grant [LP120200079]; Commonwealth of
Australia through the National Security Science and Technology Centre
within the Defence Science and Technology Group (DST Group) of the
Department of Defence; United States of America Department of Defense
through the Combating Terrorism Technical Support Office (CTTSO); DST
Group; CTTSO
FX The authors would like to acknowledge Daniel Rodriguez Estrada for the
development of Figs. 1 and 2. Lucas Blanes is supported by an Australian
Research Council Linkage Grant LP120200079.; This research was also
financially supported by the Commonwealth of Australia through the
National Security Science and Technology Centre within the Defence
Science and Technology Group (DST Group) of the Department of Defence,
and the United States of America Department of Defense through the
Combating Terrorism Technical Support Office (CTTSO). Financial support
by DST Group and CTTSO does not constitute an express or implied
endorsement of the results or conclusions of the research by the funding
organisations or their respective Departments.
NR 35
TC 4
Z9 4
U1 17
U2 54
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0021-9673
EI 1873-3778
J9 J CHROMATOGR A
JI J. Chromatogr. A
PD MAR 4
PY 2016
VL 1436
BP 28
EP 33
DI 10.1016/j.chroma.2016.01.054
PG 6
WC Biochemical Research Methods; Chemistry, Analytical
SC Biochemistry & Molecular Biology; Chemistry
GA DF9BG
UT WOS:000371654700004
PM 26850317
ER
PT J
AU Moyer, EL
Dumars, PM
Sun, GS
Martin, KJ
Heathcote, DG
Boyle, RD
Skidmore, MG
AF Moyer, Eric L.
Dumars, Paula M.
Sun, Gwo-Shing
Martin, Kara J.
Heathcote, David G.
Boyle, Richard D.
Skidmore, Mike G.
TI Evaluation of rodent spaceflight in the NASA animal enclosure module for
an extended operational period (up to 35 days)
SO NPJ MICROGRAVITY
LA English
DT Article
ID TISSUE REGENERATION; MICROGRAVITY; DIET; ARTERY; MICE
AB The National Aeronautics and Space Administration Animal Enclosure Module (AEM) was developed as a self-contained rodent habitat for shuttle flight missions that provides inhabitants with living space, food, water, ventilation, and lighting, and this study reports whether, after minimal hardware modification, the AEM could support an extended term up to 35 days for Sprague-Dawley rats and C57BL/6 female mice for use on the International Space Station. Success was evaluated based on comparison of AEM housed animals to that of vivarium housed and to normal biological ranges through various measures of animal health and well-being, including animal health evaluations, animal growth and body masses, organ masses, rodent food bar consumption, water consumption, and analysis of blood contents. The results of this study confirmed that the AEMs could support 12 adult female C57BL/6 mice for up to 35 days with self-contained RFB and water, and the AEMs could also support 5 adult male Sprague-Dawley rats for 35 days with external replenishment of diet and water. This study has demonstrated the capability and flexibility of the AEM to operate for up to 35 days with minor hardware modification. Therefore, with modifications, it is possible to utilize this hardware on the International Space Station or other operational platforms to extend the space life science research use of mice and rats.
C1 [Moyer, Eric L.; Boyle, Richard D.; Skidmore, Mike G.] NASA, Ames Res Ctr, Space Biosci Res Branch, Moffett Field, CA 94035 USA.
[Moyer, Eric L.] Blue Marble Space Inst Sci, Seattle, WA USA.
[Dumars, Paula M.; Sun, Gwo-Shing; Heathcote, David G.] NASA Res Pk, Wyle, Moffett Field, CA 94035 USA.
[Martin, Kara J.] ASRC Fed Space & Def, Beltsville, MD USA.
RP Sun, GS (reprint author), NASA Res Pk, Wyle, Moffett Field, CA 94035 USA.
EM gwo-shing.sun-1@nasa.gov
NR 21
TC 0
Z9 0
U1 1
U2 1
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 2373-8065
J9 NPJ MICROGRAVITY
JI NPJ Microgravity
PD MAR 3
PY 2016
VL 2
AR 16002
DI 10.1038/npjmgrav.2016.2
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DN9HN
UT WOS:000377390200001
ER
PT J
AU Varonen, M
Safaripour, A
Parveg, D
Kangaslahti, P
Gaier, T
Hajimiri, A
AF Varonen, M.
Safaripour, A.
Parveg, D.
Kangaslahti, P.
Gaier, T.
Hajimiri, A.
TI 200-GHz CMOS amplifier with 9-dB noise figure for atmospheric remote
sensing
SO ELECTRONICS LETTERS
LA English
DT Article
ID GHZ AMPLIFIER; DB GAIN; BAND; TECHNOLOGY
AB The feasibility of using CMOS technology for RF amplification in atmospheric remote sensing receiver is studied. The design and measurement results of a 200-GHz low-noise amplifier which is fabricated using a 32-nm SOI CMOS technology are presented. The 8-stage amplifier in a common-source configuration achieves a 9-dB noise figure and 25-dB gain with a power consumption of 33 mW.
C1 [Varonen, M.; Parveg, D.] Aalto Univ, Dept Micro & Nanosci, Espoo, Finland.
[Safaripour, A.; Hajimiri, A.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
[Kangaslahti, P.; Gaier, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Varonen, M (reprint author), Aalto Univ, Dept Micro & Nanosci, Espoo, Finland.
EM mikko.varonen@aalto.fi
FU Academy of Finland; Alfred Kordel Foundation; Jet Propulsion Laboratory,
California Institute of Technology under National Aeronautics and Space
Administration
FX This work was supported by the Academy of Finland, by Alfred Kordel
Foundation and in part by the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 12
TC 0
Z9 0
U1 0
U2 4
PU INST ENGINEERING TECHNOLOGY-IET
PI HERTFORD
PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND
SN 0013-5194
EI 1350-911X
J9 ELECTRON LETT
JI Electron. Lett.
PD MAR 3
PY 2016
VL 52
IS 5
BP 369
EP 370
DI 10.1049/el.2015.3337
PG 2
WC Engineering, Electrical & Electronic
SC Engineering
GA DF7DA
UT WOS:000371516700019
ER
PT J
AU Schumacher, SILK
Bera, PP
Lee, TJ
AF Schumacher, Sara I. L. Kokkila
Bera, Partha P.
Lee, Timothy J.
TI Characterization of the Azirinyl Cation and Its Isomers
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID FOCK PERTURBATION-THEORY; ION-MOLECULE REACTIONS; VIBRATIONAL
FREQUENCIES; SPECTROSCOPIC CONSTANTS; CYCLOPROPENYL CATION; INTERSTELLAR
CLOUDS; LINEAR C3H3+; CHEMISTRY; THERMOCHEMISTRY; ISOTOPOLOGUES
AB The azirinyl cation (C2H2N+) and its geometrical isomers could be present in the interstellar medium. The C2H2N+ isomers are, however, difficult to identify in interstellar chemistry because of the lack of high-resolution spectroscopic data from laboratory experiments. Ab initio quantum chemical methods were used to characterize the structures, relative energies, and spectroscopic and physical properties of the low energy isomers of the azirinyl.cation. We have employed second-order. Moller-Plesset perturbation. theory (MP2), second-order Z-averaged perturbation theory, (ZAPT1), and coupled cluster theory with singles and doubles with perturbative triples CCSD(T) methods along with large correlation consistent basis sets such as cc-pVTZ, cc-pCVTZ, cc-pVQZ, cc-pCVQZ, and cc-pVSZ. Harmonic vibrational frequencies, dipole moments, rotational constants, and proton affinities for the lowest energy isomers were calculated using the CCSD(T) method. Azirinyl cation, a cyclic isomer, is lowest in energy at all levels of theory employed. Azirinyl cation is followed by the cyanomethyl cation (H2CCN)(+), isocyanomethyl cation (H2CNC)(+), and a quasilinear HCCNH+ cation, which are 13.8, 17.3, and 21.5 kcal mol(-1) above the cyclic isomer, respectively, at the CCSD(T)/cc-pV5Z level of theory. The lowest three isomers all have C-2v symmetry and (1)A(1) ground electronic states. The quasilinear HCCNH+ cation has a C-s symmetry planar structure, and a (3)A '' electronic ground state, unlike what some previous work suggested.
C1 [Schumacher, Sara I. L. Kokkila; Bera, Partha P.; Lee, Timothy J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Bera, Partha P.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
[Schumacher, Sara I. L. Kokkila] Stanford Univ, Palo Alto, CA 94305 USA.
RP Lee, TJ (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
EM timothy.j.lee@nasa.gov
RI Lee, Timothy/K-2838-2012;
OI Kokkila Schumacher, Sara/0000-0002-2338-4815
FU National Aeronautics and Space Administration through the NASA
Astrobiology Institute [NNH13ZDA017C]; BAER Institute
FX This material is based upon work supported by the National Aeronautics
and Space Administration through the NASA Astrobiology Institute under
Cooperative Agreement Notice NNH13ZDA017C issued through the Science
Mission Directorate. P.P.B. acknowledges support from the BAER
Institute.
NR 47
TC 2
Z9 2
U1 2
U2 4
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD MAR 3
PY 2016
VL 120
IS 8
BP 1275
EP 1282
DI 10.1021/acs.jpca.5b12373
PG 8
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DF7UC
UT WOS:000371562100015
ER
PT J
AU Roberts, JJ
Best, BD
Mannocci, L
Fujioka, E
Halpin, PN
Palka, DL
Garrison, LP
Mullin, KD
Cole, TVN
Khan, CB
McLellan, WA
Pabst, DA
Lockhart, GG
AF Roberts, Jason J.
Best, Benjamin D.
Mannocci, Laura
Fujioka, Ei
Halpin, Patrick N.
Palka, Debra L.
Garrison, Lance P.
Mullin, Keith D.
Cole, Timothy V. N.
Khan, Christin B.
McLellan, William A.
Pabst, D. Ann
Lockhart, Gwen G.
TI Habitat-based cetacean density models for the US Atlantic and Gulf of
Mexico
SO SCIENTIFIC REPORTS
LA English
DT Article
ID MARINE MAMMALS; SUBMARINE-CANYON; SPATIAL MODELS; WHALES; ABUNDANCE;
MANAGEMENT; WATERS; RESPONSES; OCEAN
AB Cetaceans are protected worldwide but vulnerable to incidental harm from an expanding array of human activities at sea. Managing potential hazards to these highly-mobile populations increasingly requires a detailed understanding of their seasonal distributions and habitats. Pursuant to the urgent need for this knowledge for the U.S. Atlantic and Gulf of Mexico, we integrated 23 years of aerial and shipboard cetacean surveys, linked them to environmental covariates obtained from remote sensing and ocean models, and built habitat-based density models for 26 species and 3 multi-species guilds using distance sampling methodology. In the Atlantic, for 11 well-known species, model predictions resembled seasonal movement patterns previously suggested in the literature. For these we produced monthly mean density maps. For lesser-known taxa, and in the Gulf of Mexico, where seasonal movements were less well described, we produced year-round mean density maps. The results revealed high regional differences in small delphinoid densities, confirmed the importance of the continental slope to large delphinoids and of canyons and seamounts to beaked and sperm whales, and quantified seasonal shifts in the densities of migratory baleen whales. The density maps, freely available online, are the first for these regions to be published in the peer-reviewed literature.
C1 [Roberts, Jason J.; Best, Benjamin D.; Mannocci, Laura; Fujioka, Ei; Halpin, Patrick N.] Duke Univ, Nicholas Sch Environm, Marine Geospatial Ecol Lab, Durham, NC 27708 USA.
[Best, Benjamin D.] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA.
[Palka, Debra L.; Cole, Timothy V. N.; Khan, Christin B.] Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, Woods Hole, MA 02543 USA.
[Garrison, Lance P.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Miami, FL USA.
[Mullin, Keith D.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Pascagoula, MS USA.
[McLellan, William A.; Pabst, D. Ann] Univ N Carolina, Biol & Marine Biol, Wilmington, NC 28401 USA.
[Lockhart, Gwen G.] Virginia Aquarium & Marine Sci Ctr, Virginia Beach, VA USA.
RP Roberts, JJ (reprint author), Duke Univ, Nicholas Sch Environm, Marine Geospatial Ecol Lab, Durham, NC 27708 USA.
EM jason.roberts@duke.edu
FU CNES; U.S. Navy Fleet Forces Command; NASA [NNX08AK73G]; Virginia
Coastal Zone Management Program at the Department of Environmental
Quality through Task 1 of Grant [NA12NOS4190027]; NOAA [NA13NOS4190135]
FX Above all, we thank the observers, scientists, engineers, pilots,
captains, and crews who collected and shared cetacean and remote sensing
observations with us; thank you for the opportunity to analyze the data
you produced. Amy Whitt, Suzanne Bates, and Gary Buchanan contributed
the NJ-DEP surveys. Phil Hammond, Claire Lacey and colleagues
contributed the SCANS and CODA surveys. Vincent Ridoux and colleagues
contributed the REMMOA surveys. Odd Aksel Bergstad, Thomas de Lange
Wenneck, Leif Nottestad, and Gordon Waring contributed the MAR-ECO
survey under the Norwegian License for Open Government data (NLOD). The
altimeter products used in this analysis were produced by SSALTO/DUACS
and distributed by AVISO, with support from CNES
(http://www.aviso.altimetry.fr/duacs/). Dudley Chelton, Michael Schlax,
and colleagues contributed a database of geostrophic eddies detected in
the AVISO data. Stephane Maritorena and Erik Fields contributed
satellite chlorophyll data from the Ocean Color MEaSUREs project
(http://wiki.icess.ucsb.edu/measures/Products). Patrick Lehodey, Beatriz
Calmettes, and colleagues contributed zooplankton and micronekton
results from the SEAPODYM ocean model. Thanks to our colleagues for
review and advice, especially Susan Barco, Elizabeth Becker, Danielle
Cholewiak, Peter Corkeron, Andrew DiMatteo, Megan Ferguson, Karin
Forney, Jim Hain, Jolie Harrison, Leila Hatch, Dave Johnston, Elizabeth
Josephson, Erin LaBrecque, David L. Miller, Doug Nowacek, Joel
Ortega-Ortiz, Richard Pace, Rui Prieto, Andy Read, Denise Risch, Jooke
Robbins, Rob Schick, Doug Sigourney, Melissa Soldevilla, Joy
Stanistreet, Len Thomas, Kim Urian, Sofie Van Parijs, Danielle Waples,
and Simon Wood. Funding for this analysis was provided by the U.S. Navy
Fleet Forces Command and by NASA (Grant/Cooperative Agreement Number
NNX08AK73G). The VAMSC aerial surveys were funded by the Virginia
Coastal Zone Management Program at the Department of Environmental
Quality through Task 1 of Grant NA12NOS4190027 and Task 95.02 of Grant
NA13NOS4190135 from NOAA, under the Coastal Zone Management Act of 1972,
as amended. The NOAA GOM aerial and ship surveys were primarily
conducted under inter-agency agreements between SEFSC and BOEM Gulf of
Mexico Region (numbers 16197, 1445-IA09-96-0009, and 15958). The UNCW
Navy surveys were funded by U.S. Navy Fleet Forces Command with Joel
Bell as the COTR. The UNCW right whale surveys were funded by NOAA. The
Navy was given the opportunity to suggest spatial, temporal, and
taxonomical resolutions and a geographic extent that would facilitate
the Navy's use of the results in U.S. environmental regulatory
processes. When the analysis was complete, the Navy was given
opportunity to view preliminary results. No funders, including the Navy,
participated in the analysis of the data or the preparation of the
manuscript.
NR 57
TC 1
Z9 1
U1 13
U2 26
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD MAR 3
PY 2016
VL 6
AR 22615
DI 10.1038/srep22615
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DF3AB
UT WOS:000371215000001
PM 26936335
ER
PT J
AU Yanovsky, I
Lambrigtsen, BH
AF Yanovsky, Igor
Lambrigtsen, Bjorn H.
TI Enhancing the temporal resolution of image sequences capturing evolving
weather phenomena
SO REMOTE SENSING LETTERS
LA English
DT Article
ID ALGORITHMS; RADIOMETER
AB In this article, we develop an approach for temporal resolution enhancement of blurry and distorted image sequences capturing evolving weather phenomena. We first enhance the spatial resolution of a sequence of images using an efficient deconvolution method which we showed to reduce image ringing, blurring, and distortion, while sharpening the image and preserving information content. Such methodology is based on current research in sparse optimization and compressed sensing, which lead to unprecedented efficiencies for solving image reconstruction problems. We then consider the evolving sequence to be embedded in a deformable medium, and enhance temporal resolution of a sequence using nonlinear viscous fluid registration model. The physical continuum equation is solved using an efficient multigrid full approximation scheme.
C1 [Yanovsky, Igor; Lambrigtsen, Bjorn H.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
RP Yanovsky, I (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
EM igor.yanovsky@jpl.nasa.gov
FU National Science Foundation [DMS 1217239]
FX The research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. IY also acknowledges support from
the National Science Foundation [grant number DMS 1217239].
NR 15
TC 0
Z9 0
U1 1
U2 8
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 2150-704X
EI 2150-7058
J9 REMOTE SENS LETT
JI Remote Sens. Lett.
PD MAR 3
PY 2016
VL 7
IS 3
BP 239
EP 248
DI 10.1080/2150704X.2015.1128130
PG 10
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA CZ2VT
UT WOS:000366963400001
ER
PT J
AU Kolodziejska, JA
Kozachkov, H
Kranjc, K
Hunter, A
Marquis, E
Johnson, WL
Flores, KM
Hofmann, DC
AF Kolodziejska, Joanna A.
Kozachkov, Henry
Kranjc, Kelly
Hunter, Allen
Marquis, Emmanuelle
Johnson, William L.
Flores, Katharine M.
Hofmann, Douglas C.
TI Towards an understanding of tensile deformation in Ti-based bulk
metallic glass matrix composites with BCC dendrites
SO SCIENTIFIC REPORTS
LA English
DT Article
ID MECHANICAL-PROPERTIES; DUCTILITY; PHASE; DISPERSIONS; SHEAR
AB The microstructure and tension ductility of a series of Ti-based bulk metallic glass matrix composite (BMGMC) is investigated by changing content of the beta stabilizing element vanadium while holding the volume fraction of dendritic phase constant. The ability to change only one variable in these novel composites has previously been difficult, leading to uninvestigated areas regarding how composition affects properties. It is shown that the tension ductility can range from near zero percent to over ten percent simply by changing the amount of vanadium in the dendritic phase. This approach may prove useful for the future development of these alloys, which have largely been developed experimentally using trial and error.
C1 [Kolodziejska, Joanna A.; Kozachkov, Henry; Johnson, William L.] CALTECH, Keck Lab Engn, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
[Kranjc, Kelly; Flores, Katharine M.] Washington Univ, Dept Mech Engn & Mat Sci, Inst Mat Sci & Engn, 1 Brookings Dr,Campus Box 1185, St Louis, MO 63130 USA.
[Hunter, Allen; Marquis, Emmanuelle] Univ Michigan, Dept Mat Sci & Engn, Ann Arbor, MI 48109 USA.
[Hofmann, Douglas C.] CALTECH, Jet Prop Lab, Mat Dev & Mfg Technol, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Hofmann, DC (reprint author), CALTECH, Jet Prop Lab, Mat Dev & Mfg Technol, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM dch@jpl.nasa.gov
OI Marquis, Emmanuelle/0000-0002-6476-2835
FU Air Force Office of Scientific Research [FA9550-09-1-0251,
FA9550-12-1-0059]
FX This work was supported by the Air Force Office of Scientific Research
under Grant Nos. FA9550-09-1-0251 and FA9550-12-1-0059. Part of this
work was done at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration (NASA).
NR 19
TC 8
Z9 9
U1 13
U2 42
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD MAR 2
PY 2016
VL 6
AR 22563
DI 10.1038/srep22563
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DF2DI
UT WOS:000371150000001
PM 26932509
ER
PT J
AU Edberg, SJ
Evans, DL
Graf, JE
Hyon, JJ
Rosen, PA
Waliser, DE
AF Edberg, Stephen J.
Evans, Diane L.
Graf, James E.
Hyon, Jason J.
Rosen, Paul A.
Waliser, Duane E.
TI Studying Earth in the New Millennium NASA Jet Propulsion Laboratory's
Contributions to Earth Science and Applications
SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE
LA English
DT Article
ID AQUARIUS/SAC-D MISSION; OBSERVING SYSTEM; AURA SATELLITE; SPECTROMETER;
SALINITY; SOUNDER
C1 [Edberg, Stephen J.; Evans, Diane L.; Graf, James E.; Hyon, Jason J.; Rosen, Paul A.; Waliser, Duane E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
RP Edberg, SJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM stephen.j.edberg@jpl.nasa.gov; diane.l.evans@jpl.nasa.gov;
james.e.graf@jpl.nasa.gov; jason.j.hyon@jpl.nasa.gov;
paul.a.rosen@jpl.nasa.gov; duane.e.waliser@jpl.nasa.gov
NR 52
TC 0
Z9 0
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2168-6831
J9 IEEE GEOSC REM SEN M
JI IEEE Geosci. Remote Sens. Mag.
PD MAR
PY 2016
VL 4
IS 1
BP 26
EP 39
DI 10.1109/MGRS.2016.2525678
PG 14
WC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
SC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
GA EF0HL
UT WOS:000390006400004
ER
PT J
AU Spencer, M
Ulaby, F
AF Spencer, Michael
Ulaby, Fawwaz
TI Spectrum Issues Faced by Active Remote Sensing Radio frequency
interference and operational restrictions
SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE
LA English
DT Article
C1 [Spencer, Michael] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Ulaby, Fawwaz] Univ Michigan, Ann Arbor, MI 48109 USA.
RP Spencer, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2168-6831
J9 IEEE GEOSC REM SEN M
JI IEEE Geosci. Remote Sens. Mag.
PD MAR
PY 2016
VL 4
IS 1
BP 40
EP 45
DI 10.1109/MGRS.2016.2517410
PG 6
WC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
SC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
GA EF0HL
UT WOS:000390006400005
ER
PT J
AU Kruk, JW
Xapsos, MA
Armani, N
Stauffer, C
Hirata, CM
AF Kruk, Jeffrey W.
Xapsos, Michael A.
Armani, Nerses
Stauffer, Craig
Hirata, Christopher M.
TI Radiation-induced Backgrounds in Astronomical Instruments:
Considerations for Geosynchronous Orbit and Implications for the Design
of the WFIRST Wide-field Instrument
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE instrumentation: detectors; instrumentation: miscellaneous; space
vehicles: instruments
ID COLLISION STOPPING POWER; CHARGED-PARTICLES; SPACE; POSITRONS;
ELECTRONS; ELEMENTS
AB Geosynchronous orbits are appealing for solar or astrophysical observatories because they permit continuous data downlink at high rates. The radiation environment in these orbits presents unique challenges, however. This paper describes both the characteristics of the radiation environment in geosynchronous orbit and the mechanisms by which this radiation generates backgrounds in photon detectors. Shielding considerations are described, and a preliminary shielding design for the proposed Wide-Field InfraRed Survey Telescope. observatory is presented as a reference for future space telescope concept studies that consider a geosynchronous orbit.
C1 [Kruk, Jeffrey W.; Xapsos, Michael A.; Armani, Nerses; Stauffer, Craig] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hirata, Christopher M.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys CCAPP, 191 West Woodruff Ave, Columbus, OH 43210 USA.
RP Kruk, JW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Jeffrey.W.Kruk@nasa.gov
FU WFIRST Study Office at NASA/GSFC; David and Lucile Packard Foundation;
Simons Foundation; U.S. Department of Energy
FX The authors would like to thank the anonymous referee for numerous
comments that improved the clarity of presentation throughout the paper.
The authors would like to thank Tom Jordan for numerous discussions on
usage of the NOVICE code for our application, and one of us (J.W.K.)
wishes to thank Bernie Rauscher for a number of useful discussions on
detector architecture. This work made use of data on the geosynchronous
orbit environment obtained by the EPEAD instrument on the GOES-13.
satellite, and provided via the National Geophysical Data Center
operated by NOAA. We made use of energy loss tables from the NIST
Standard Reference Database 124
(http://www.nist.gov/pml/data/star/index.cfm) and photon cross sections
from the NIST XCOM database
(http://www.nist.gov/pml/data/xcom/index.cfm). This work was supported
by the WFIRST Study Office at NASA/GSFC. C.H. is supported by the David
and Lucile Packard Foundation, the Simons Foundation, and the U.S.
Department of Energy.
NR 27
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD MAR
PY 2016
VL 128
IS 961
AR 035005
DI 10.1088/1538-3873/128/961/035005
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EB1JM
UT WOS:000387107100007
ER
PT J
AU Fadel, TR
Farrell, DF
Friedersdorf, LE
Griep, MH
Hoover, MD
Meador, MA
Meyyappan, M
AF Fadel, Tarek R.
Farrell, Dorothy F.
Friedersdorf, Lisa E.
Griep, Mark H.
Hoover, Mark D.
Meador, Michael A.
Meyyappan, M.
TI Toward the Responsible Development and Commercialization of Sensor
Nanotechnologies
SO ACS SENSORS
LA English
DT Article
DE nanosensors; engineered nanomaterials; commercialization; data quality;
life cycle
ID CARBON NANOTUBES; NANOPORE SENSORS; DNA; NANOPARTICLES; GRAPHENE;
NANOMATERIALS; NANOSENSORS; TRANSISTOR; MOLECULES; SYSTEM
AB Nanotechnology-enabled sensors (or nano sensors) will play an important role in enabling the progression toward ubiquitous information systems as the Internet of Things (IoT) emerges. Nanosensors offer new, miniaturized solutions in physiochemical and biological sensing that enable increased sensitivity, specificity, and multiplexing capability, all with the compelling economic drivers of low cost and high-energy efficiency. In the United States, Federal agencies participating in the National Nano technology Initiative (NNI) "Nanotechnology for Sensors and Sensors for Nanotechnology: Improving and Protecting Health, Safety, and the Environment" Nanotechnology Signature Initiative (the Sensors NSI), address both the opportunity of using nanotechnology to advance sensor development and the challenges of developing sensors to keep pace with the increasingly widespread use of engineered nanomaterials. This perspective article will introduce and provide background on the NNI signature initiative on sensors. Recent efforts by the Sensors NSI aimed at promoting the successful development and commercialization of nanosensors will be reviewed and examples of sensor nanotechnologies will be highlighted. Future directions and critical challenges for sensor development will also be discussed.
C1 [Fadel, Tarek R.; Friedersdorf, Lisa E.; Meador, Michael A.] Natl Nanotechnol Coordinat Off, 4201 Wilson Blvd,Suite 405, Arlington, VA 22230 USA.
[Farrell, Dorothy F.] NCI, NIH, 31 Ctr Dr,10A52, Bethesda, MD 20892 USA.
[Griep, Mark H.] US Army, Res Lab, Aberdeen, MD 21005 USA.
[Hoover, Mark D.] NIOSH, 1095 Willowdale Rd, Morgantown, WV 26505 USA.
[Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
RP Fadel, TR (reprint author), Natl Nanotechnol Coordinat Off, 4201 Wilson Blvd,Suite 405, Arlington, VA 22230 USA.
EM TFadel@nnco.nano.gov
NR 76
TC 1
Z9 1
U1 6
U2 6
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 2379-3694
J9 ACS SENSORS
JI ACS Sens.
PD MAR
PY 2016
VL 1
IS 3
BP 207
EP 216
DI 10.1021/acssensors.5b00279
PG 10
WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology
SC Chemistry; Science & Technology - Other Topics
GA DY9OT
UT WOS:000385464400002
PM 28261665
ER
PT J
AU Youngquist, RC
Nurge, MA
Starr, SO
Leve, FA
Peck, M
AF Youngquist, Robert C.
Nurge, Mark A.
Starr, Stanley O.
Leve, Frederick A.
Peck, Mason
TI A slowly rotating hollow sphere in a magnetic field: First steps to
de-spin a space object
SO AMERICAN JOURNAL OF PHYSICS
LA English
DT Article
ID DEBRIS
AB Modeling the interaction of a slowly rotating hollow conducting sphere in a magnetic field provided an understanding of the dynamics of orbiting space objects moving through the Earth's magnetic field. This analysis, performed in the late 1950s and limited to uniform magnetic fields, was innovative and acknowledged the pioneers who first observed rotary magnetism, in particular, the seminal work of Hertz in 1880. Now, there is interest in using a magnetic field produced by one space object to stop the spin of a second object so that docking can occur. In this paper, we consider, yet again, the interaction of a rotating hollow sphere in a magnetic field. We show that the predicted results can be tested experimentally, making this an interesting advanced student project. This analysis also sheds light on a rich set of previously unaddressed behaviors involving eddy currents. (C) 2016 American Association of Physics Teachers.
C1 [Youngquist, Robert C.; Nurge, Mark A.; Starr, Stanley O.] NASA, Mail Code UBR3, Kennedy Space Ctr, FL 32899 USA.
[Leve, Frederick A.] Air Force Res Lab, Kirtland AFB, NM 87117 USA.
[Peck, Mason] Cornell Univ, Sibley Sch Mech & Aerosp Engn, 208 Upson Hall,124 Hoy Rd, Ithaca, NY 14853 USA.
RP Nurge, MA (reprint author), NASA, Mail Code UBR3, Kennedy Space Ctr, FL 32899 USA.
EM Robert.C.Yougquist@nasa.gov; Mark.A.Nurge@nasa.gov;
Stanley.O.Starr@nasa.gov; frederick.leve@us.af.mil; mp336@cornell.edu
NR 23
TC 0
Z9 0
U1 1
U2 1
PU AMER ASSOC PHYSICS TEACHERS
PI COLLEGE PARK
PA ONE PHYSICS ELLIPSE, COLLEGE PARK, MD 20740-3845 USA
SN 0002-9505
EI 1943-2909
J9 AM J PHYS
JI Am. J. Phys.
PD MAR
PY 2016
VL 84
IS 3
BP 181
EP 191
DI 10.1119/1.4936633
PG 11
WC Education, Scientific Disciplines; Physics, Multidisciplinary
SC Education & Educational Research; Physics
GA DX9SF
UT WOS:000384734700002
ER
PT J
AU Pesnell, WD
AF Pesnell, W. Dean
TI Flying through polytropes
SO AMERICAN JOURNAL OF PHYSICS
LA English
DT Article
ID 40 MINUTES; EARTH; SPHERES
AB Dropping objects into a tunnel bored through Earth has been used to visualize simple harmonic motion for many years, and even imagined for use as rapid transport systems. Unlike previous studies that assumed a constant density Earth, here we calculate the fall-through time of polytropes, models of Earth's interior where the pressure varies as a power of the density. This means the fall-through time can be calculated as the central condensation varies from one to large within the family of polytropes. Having a family of models, rather than a single model, helps to explore the properties of planets and stars. Comparing the family of phase space solutions shows that the fall-through time and velocity approach the limit of radial free-fall onto a point mass as the central condensation increases. More condensed models give higher maximum velocities but do not have the right global properties for Earth. The angular distance one can travel along the surface is calculated as a brachistochrone (path of least time) tunnel that is a function of the depth to which the tunnel is bored. We also show that completely degenerate objects, simple models of white dwarf stars supported by completely degenerate electrons, have sizes similar to Earth but their much higher masses mean a much larger gravitational strength and a shorter fall-through time. Numerical integrations of the equations describing polytropes and completely degenerate objects are used to generate the initial models. Analytic solutions and numerical integration of the equations of motion are used to calculate the fall-through time for each model, and numerical integrations with analytic approximations at the boundaries are used to calculate the brachistochrones in the polytropes. Scaling relationships are provided to help use these results in other planets and stars. (C) 2016 American Association of Physics Teachers.
C1 [Pesnell, W. Dean] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Pesnell, WD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM William.D.Pesnell@NASA.gov
FU NASA's Solar Dynamics Observatory
FX The authors gratefully acknowledge the support of NASA's Solar Dynamics
Observatory. The comments of the referees were useful in clarifying the
discussion of the fall-through time calculation.
NR 29
TC 0
Z9 0
U1 0
U2 0
PU AMER ASSOC PHYSICS TEACHERS
PI COLLEGE PARK
PA ONE PHYSICS ELLIPSE, COLLEGE PARK, MD 20740-3845 USA
SN 0002-9505
EI 1943-2909
J9 AM J PHYS
JI Am. J. Phys.
PD MAR
PY 2016
VL 84
IS 3
BP 192
EP 201
DI 10.1119/1.4939574
PG 10
WC Education, Scientific Disciplines; Physics, Multidisciplinary
SC Education & Educational Research; Physics
GA DX9SF
UT WOS:000384734700003
ER
PT J
AU Comfort, N
AF Comfort, Nathaniel
TI Eclipse of Man: Human Extinction and the Meaning of Progress
SO ISSUES IN SCIENCE AND TECHNOLOGY
LA English
DT Book Review
C1 [Comfort, Nathaniel] Johns Hopkins Univ, NASA, Lib Congress, Astrobiol, Baltimore, MD 21218 USA.
[Comfort, Nathaniel] Johns Hopkins Univ, Inst Hist Med, Baltimore, MD 21218 USA.
RP Comfort, N (reprint author), Johns Hopkins Univ, NASA, Lib Congress, Astrobiol, Baltimore, MD 21218 USA.; Comfort, N (reprint author), Johns Hopkins Univ, Inst Hist Med, Baltimore, MD 21218 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0748-5492
EI 1938-1557
J9 ISSUES SCI TECHNOL
JI Issues Sci. Technol.
PD SPR
PY 2016
VL 32
IS 3
BP 91
EP +
PG 3
WC Engineering, Multidisciplinary; Engineering, Industrial;
Multidisciplinary Sciences; Social Issues
SC Engineering; Science & Technology - Other Topics; Social Issues
GA DX9IM
UT WOS:000384706800035
ER
PT J
AU Holzmann, GJ
AF Holzmann, Gerard J.
TI Code Clarity
SO IEEE SOFTWARE
LA English
DT Article
C1 [Holzmann, Gerard J.] NASA, Jet Prop Lab, Washington, DC 20546 USA.
RP Holzmann, GJ (reprint author), NASA, Jet Prop Lab, Washington, DC 20546 USA.
EM gholzmann@acm.org
NR 1
TC 0
Z9 0
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0740-7459
EI 1937-4194
J9 IEEE SOFTWARE
JI IEEE Softw.
PD MAR-APR
PY 2016
VL 33
IS 2
BP 22
EP 25
PG 4
WC Computer Science, Software Engineering
SC Computer Science
GA DV7BT
UT WOS:000383091700006
ER
PT J
AU Lolli, S
Lewis, JR
Campbell, JR
Welton, EJ
Gu, Y
AF Lolli, S.
Lewis, J. R.
Campbell, J. R.
Welton, E. J.
Gu, Y.
TI Cirrus cloud radiative characteristics from continuous MPLNET profiling
at GSFC in 2012
SO OPTICA PURA Y APLICADA
LA English
DT Article
DE Lidar; Cirrus Clouds; Extinction coefficient; Radiative Transfer;
Climate change
ID RETRIEVALS; SCATTERING
AB Optically thin cirrus cloud (optical depth < 0.03) net radiative effect represents one of the primary uncertainties in climate feedback, as sub-visible clouds play a fundamental role in atmospheric radiation balance and climate change. A lidar is a very sensitive optical device to detect clouds with an optical depth as low as 10(-4). In this paper we assess the daytime net radiative effect of sub-visible cirrus clouds detected at Goddard Space Flight Center, a permanent observational site of the NASA Micro Pulse Lidar Network in 2012. Depending on their height, season and hour of the day, the solar albedo effect can outweigh the infrared greenhouse effect, cooling the earth-atmosphere system rather than warming it exclusively. As result, based on latitude, the net effect of sub-visible cirrus clouds can be more accurately parameterized in climate models.
C1 [Lolli, S.; Lewis, J. R.] NASA GSFC JCET, Code 612, Greenbelt, MD 20771 USA.
[Campbell, J. R.] US Navy, Res Lab, Monterey, CA 93943 USA.
[Welton, E. J.] NASA GSFC, Code 612, Greenbelt, MD 20771 USA.
[Gu, Y.] UCLA, Los Angeles, CA USA.
RP Lolli, S (reprint author), NASA GSFC JCET, Code 612, Greenbelt, MD 20771 USA.
EM simone.lolli@nasa.gov
NR 16
TC 1
Z9 1
U1 0
U2 0
PU SOC ESPANOLA OPTICA
PI MADRID
PA SERRANO, 121, MADRID, 28006, SPAIN
SN 0030-3917
EI 2171-8814
J9 OPT PURA APL
JI Opt. Pura Apl.
PD MAR
PY 2016
VL 49
IS 1
BP 1
EP 6
DI 10.7149/OPA.49.1.1
PG 6
WC Optics
SC Optics
GA DV2ZL
UT WOS:000382790700002
ER
PT J
AU Wei, JW
Lee, ZP
Ondrusek, M
Mannino, A
Tzortziou, M
Armstrong, R
AF Wei, Jianwei
Lee, Zhongping
Ondrusek, Michael
Mannino, Antonio
Tzortziou, Maria
Armstrong, Roy
TI Spectral slopes of the absorption coefficient of colored dissolved and
detrital material inverted from UV-visible remote sensing reflectance
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID INHERENT OPTICAL-PROPERTIES; ORGANIC-MATTER CDOM; QUASI-ANALYTICAL
ALGORITHM; WATER-LEAVING RADIANCE; OCEAN COLOR; MISSISSIPPI RIVER;
ATMOSPHERIC CORRECTION; ULTRAVIOLET-RADIATION; GLOBAL DISTRIBUTION;
CONTINENTAL-SHELF
AB The spectral slope of the absorption coefficient of colored dissolved and detrital material (CDM), S-cdm (units: nm(-1)), is an important optical parameter for characterizing the absorption spectral shape of CDM. Although highly variable in natural waters, in most remote sensing algorithms, this slope is either kept as a constant or empirically modeled with multiband ocean color in the visible domain. In this study, we explore the potential of semianalytically retrieving S-cdm with added ocean color information in the ultraviolet (UV) range between 360 and 400 nm. Unique features of hyperspectral remote sensing reflectance in the UV-visible wavelengths (360-500 nm) have been observed in various waters across a range of coastal and open ocean environments. Our data and analyses indicate that ocean color in the UV domain is particularly sensitive to the variation of the CDM spectral slope. Here, we used a synthesized dataset to show that adding UV wavelengths to the ocean color measurements will improve the retrieval of S-cdm from remote sensing reflectance considerably, while the spectral band settings of past and current satellite ocean color sensors cannot fully account for the spectral variation of remote sensing reflectance. Results of this effort support the concept to include UV wavelengths in the next generation of satellite ocean color sensors.
C1 [Wei, Jianwei; Lee, Zhongping] Univ Massachusetts, Sch Environm, Opt Oceanog Lab, Boston, MA 02125 USA.
[Ondrusek, Michael] NOAA, NESDIS Ctr Weather & Climate Predict, College Pk, MD USA.
[Mannino, Antonio] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD USA.
[Tzortziou, Maria] CUNY City Coll, Dept Earth & Atmospher Sci, New York, NY 10031 USA.
[Armstrong, Roy] Univ Puerto Rico, Bioopt Oceanog Lab, Mayaguez, PR USA.
RP Wei, JW (reprint author), Univ Massachusetts, Sch Environm, Opt Oceanog Lab, Boston, MA 02125 USA.
EM jianwei.wei@umb.edu
RI Ondrusek, Michael/F-5617-2010; Mannino, Antonio/I-3633-2014
OI Ondrusek, Michael/0000-0002-5311-9094;
FU National Aeronautics and Space Administration (NASA) Ocean Biology and
Biogeochemistry and Water and Energy Cycle Programs; GEO-CAPE project;
National Oceanic and Atmospheric Administration (NOAA) JPSS VIIRS Ocean
Color Cal/Val Project
FX Financial support by the National Aeronautics and Space Administration
(NASA) Ocean Biology and Biogeochemistry and Water and Energy Cycle
Programs, the GEO-CAPE project, and the National Oceanic and Atmospheric
Administration (NOAA) JPSS VIIRS Ocean Color Cal/Val Project is greatly
appreciated. The Rrs data in the North Pacific Gyre were collected by
Marlon Lewis at the Dalhousie University. We thank Emmanuel Boss and an
anonymous reviewer for comments and suggestions, which have improved the
manuscript.
NR 80
TC 3
Z9 3
U1 6
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD MAR
PY 2016
VL 121
IS 3
BP 1953
EP 1969
DI 10.1002/2015JC011415
PG 17
WC Oceanography
SC Oceanography
GA DO8YY
UT WOS:000378072700026
ER
PT J
AU Bushnell, DM
Moses, RW
AF Bushnell, Dennis M.
Moses, Robert W.
TI FRESH THINKING ABOUT MARS
SO AEROSPACE AMERICA
LA English
DT Article
C1 [Bushnell, Dennis M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Moses, Robert W.] Langley, Hampton, VA USA.
[Moses, Robert W.] ISRU, Off Chief Engineer, Syst Capabilities Leadership Team, Hampton, VA USA.
[Moses, Robert W.] AIAA, Reston, VA USA.
RP Bushnell, DM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM dennis.m.bushnell@nasa.gov; robert.w.moses@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0740-722X
J9 AEROSPACE AM
JI Aerosp. Am.
PD MAR
PY 2016
VL 54
IS 3
BP 34
EP 39
PG 6
WC Engineering, Aerospace
SC Engineering
GA DO4RJ
UT WOS:000377770400006
ER
PT J
AU Risacher, C
Gusten, R
Stutzki, J
Hubers, HW
Buchel, D
Graf, UU
Heyminck, S
Honingh, CE
Jacobs, K
Klein, B
Klein, T
Leinz, C
Putz, P
Reyes, N
Ricken, O
Wunsch, HJ
Fusco, P
Rosner, S
AF Risacher, Christophe
Guesten, Rolf
Stutzki, Juergen
Huebers, Heinz-Wilhelm
Buechel, Denis
Graf, Urs U.
Heyminck, Stefan
Honingh, Cornelia E.
Jacobs, Karl
Klein, Bernd
Klein, Thomas
Leinz, Christian
Puetz, Patrick
Reyes, Nicolas
Ricken, Oliver
Wunsch, Hans-Joachim
Fusco, Paul
Rosner, Stefan
TI First Supra-THz Heterodyne Array Receivers for Astronomy With the SOFIA
Observatory
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Cryogenics; far-infrared astronomy; HEB mixer; heterodyne; receivers;
submillimeter-wave technology; superconducting devices
ID QUANTUM CASCADE LASER; PULSE TUBE COOLER; LOCAL OSCILLATOR; BOLOMETER
CAMERA; 4 K; TERAHERTZ; TELESCOPE; NOISE; MIXER
AB We present the upGREAT THz heterodyne arrays for far-infrared astronomy. The low-frequency array (LFA) is designed to cover the 1.9-2.5 THz range using 2 7-pixel wave-guide-based HEB mixer arrays in a dual polarization configuration. The high-frequency array (HFA) will perform observations of the [OI] line at 4.745 THz using a 7-pixel waveguide-based HEB mixer array. This paper describes the common design for both arrays, cooled to 4.5 K using closed-cycle pulse tube technology. We then show the laboratory and telescope characterization of the first array with its 14 pixels (LFA), which culminated in the successful commissioning in May 2015 aboard the SOFIA airborne observatory observing the [CII] fine structure transition at 1.9005 THz. This is the first successful demonstration of astronomical observations with a heterodyne focal plane array above 1 THz and is also the first time high-power closed-cycle coolers for temperatures below 4.5 K are operated on an airborne platform.
C1 [Risacher, Christophe; Guesten, Rolf; Heyminck, Stefan; Klein, Bernd; Klein, Thomas; Reyes, Nicolas; Ricken, Oliver] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Stutzki, Juergen; Buechel, Denis; Graf, Urs U.; Honingh, Cornelia E.; Jacobs, Karl; Puetz, Patrick] Univ Cologne, D-50937 Cologne, Germany.
[Huebers, Heinz-Wilhelm] German Aerosp Ctr DLR, Inst Opt Sensor Syst, D-12489 Berlin, Germany.
[Klein, Bernd] Univ Appl Sci Bonn Rhein Sieg, D-53757 St Augustin, Germany.
[Klein, Thomas] European Southern Observat, Vitacura 19001, Santiago De Chi, Chile.
[Reyes, Nicolas] Univ Chile, Santiago, Chile.
[Fusco, Paul] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rosner, Stefan] SETI Inst, Mountain View, CA 94043 USA.
RP Risacher, C (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM crisache@mpifr.de; stutzki@ph1.uni-koeln.de;
Heinz-Wilhelm.Hue-bers@dlr.de; bklein@mpifr.de; tklein@eso.org;
nireyes@u.uchile.cl; paul.r.fusco@nasa.gov; stefan.rosner@nasa.gov
RI Reyes, Nicolas/H-9622-2013
FU Federal Ministry of Economics and Technology via the German Space Agency
(DLR) [50 OK 1102, 50 OK 1103, 50 OK 1104]; Collaborative Research
Council 956 - Deutsche Forschungsgemeinschaft (DFG)
FX This work was supported in part by the Federal Ministry of Economics and
Technology via the German Space Agency (DLR) under Grant 50 OK 1102,
Grant 50 OK 1103, and Grant 50 OK 1104 and by the Collaborative Research
Council 956, sub-projects D3 and S, funded by the Deutsche
Forschungsgemeinschaft (DFG).
NR 41
TC 2
Z9 3
U1 5
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD MAR
PY 2016
VL 6
IS 2
BP 199
EP 211
DI 10.1109/TTHZ.2015.2508005
PG 13
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA DO3LP
UT WOS:000377683400004
ER
PT J
AU Kiuru, T
Chattopadhyay, G
Reck, TJ
Minnich, AJ
Lin, R
Schlecht, E
Siles, JV
Lee, C
Mehdi, I
AF Kiuru, Tero
Chattopadhyay, Goutam
Reck, Theodore J.
Minnich, Austin J.
Lin, Robert
Schlecht, Erich
Siles, Jose V.
Lee, Choonsup
Mehdi, Imran
TI Thermal Characterization of Substrate Options for High-Power THz
Multipliers Over a Broad Temperature Range
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Cryogenic; frequency multiplier; Schottky diode; terahertz (THz)
ID SEMICONDUCTOR-DEVICES; FREQUENCY-MULTIPLIERS; SCHOTTKY DIODES; WAVE;
VARACTORS; DESIGN; MODELS; BAND
AB This paper presents thermal characterization results for three high-power THz Schottky frequency multipliers in the temperature range of 20-380 K. All measured multipliers have different substrates: a 5-mu m-thick GaAs membrane, a 40-mu m-thick GaAs substrate, and a 5-mu m-thick GaAs membrane glued to a 20-mu m-thick CVD diamond substrate with polymer bonding agent. The thermal characterization results include such parameters as the maximum average junction temperature of the anodes, device total thermal resistance, and device cooling (or heating) times. The results enable designers to better optimize their devices for the maximum power level and temperature range and system engineers to better predict the overall performance of the system in an environment, where the ambient conditions might change. For example, from the thermal resistance point of view the GaAs membrane on diamond substrate clearly outperforms the device on GaAs membrane alone at room temperature or above. However, perhaps surprisingly, at temperatures below 125 K, the GaAs membrane is on par, or even has lower thermal resistance than the membrane on diamond.
C1 [Kiuru, Tero] VTT Tech Res Ctr Finland Ltd, MilliLab, FI-00045 Espoo, Finland.
[Minnich, Austin J.] CALTECH, Pasadena, CA 91125 USA.
[Chattopadhyay, Goutam; Reck, Theodore J.; Lin, Robert; Schlecht, Erich; Siles, Jose V.; Lee, Choonsup; Mehdi, Imran] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Kiuru, T (reprint author), VTT Tech Res Ctr Finland Ltd, MilliLab, FI-00045 Espoo, Finland.
EM tero.kiuru@vtt.fi
FU Academy of Finland
FX This work was supported in part by the Academy of Finland. The work was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, Pasadena, CA, USA under a contract with the National
Aeronautics and Space Administration (NASA)
NR 32
TC 1
Z9 1
U1 1
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD MAR
PY 2016
VL 6
IS 2
BP 328
EP 335
DI 10.1109/TTHZ.2015.2511746
PG 8
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA DO3LP
UT WOS:000377683400018
ER
PT J
AU Ghosh, P
Behnke, BJ
Stabley, JN
Kilar, CR
Park, Y
Narayanan, A
Alwood, JS
Shirazi-Fard, Y
Schreurs, AS
Globus, RK
Delp, MD
AF Ghosh, Payal
Behnke, Brad J.
Stabley, John N.
Kilar, Cody R.
Park, Yoonjung
Narayanan, Anand
Alwood, Joshua S.
Shirazi-Fard, Yasaman
Schreurs, Ann-Sofie
Globus, Ruth K.
Delp, Michael D.
TI Effects of High-LET Radiation Exposure and Hindlimb Unloading on
Skeletal Muscle Resistance Artery Vasomotor Properties and Cancellous
Bone Microarchitecture in Mice
SO RADIATION RESEARCH
LA English
DT Article
ID ENDOTHELIUM-DEPENDENT VASODILATION; SHORT-DURATION SPACEFLIGHT;
SIMULATED MICROGRAVITY; IONIZING-RADIATION; BLOOD-FLOW; VASOCONSTRICTOR
RESPONSIVENESS; ORTHOSTATIC INTOLERANCE; SPACE EXPLORATION;
XANTHINE-OXIDASE; OXIDATIVE STRESS
AB Weightlessness during spaceflight leads to functional changes in resistance arteries and loss of cancellous bone, which may be potentiated by radiation exposure. The purpose of this study was to assess the effects of hindlimb unloading (HU) and total-body irradiation (TBI) on the vasomotor responses of skeletal muscle arteries. Male C57BL/6 mice were assigned to control, HU (13-16 days), TBI (1 Gy Fe-56, 600 MeV, 10 cGy/min) and HU-TBI groups. Gastrocnemius muscle feed arteries were isolated for in vitro study. Endothelium-dependent (acetylcholine) and -independent (Dea-NONOate) vasodilator and vasoconstrictor (KCl, phenylephrine and myogenic) responses were evaluated. Arterial endothelial nitric oxide synthase (eNOS), superoxide dismutase-1 (SOD-1) and xanthine oxidase (XO) protein content and tibial cancellous bone microarchitecture were quantified. Endothelium-dependent and -independent vasodilator responses were impaired in all groups relative to control, and acetylcholine-induced vasodilation was lower in the HU-TBI group relative to that in the HU and TBI groups. Reductions in endothelium-dependent vasodilation correlated with a lower cancellous bone volume fraction. Nitric oxide synthase inhibition abolished all group differences in endothelium-dependent vasodilation. HU and HU-TBI resulted in decreases in eNOS protein levels, while TBI and HU-TBI produced lower SOD-1 and higher XO protein content. Vasoconstrictor responses were not altered. Reductions in NO bioavailability (eNOS), lower anti-oxidant capacity (SOD-1) and higher pro-oxidant capacity (XO) may contribute to the deficits in NOS signaling in skeletal muscle resistance arteries. These findings suggest that the combination of insults experienced in spaceflight leads to impairment of vasodilator function in resistance arteries that is mediated through deficits in NOS signaling. (C) 2016 by Radiation Research Society
C1 [Ghosh, Payal; Delp, Michael D.] Florida State Univ, Dept Nutr Food & Exercise Sci, Tallahassee, FL 32306 USA.
[Behnke, Brad J.] Kansas State Univ, Dept Kinesiol, Manhattan, KS 66506 USA.
[Behnke, Brad J.] Kansas State Univ, Johnson Canc Res Ctr, Manhattan, KS 66506 USA.
[Stabley, John N.] Univ Texas SW Med Ctr Dallas, Dept Internal Med, Dallas, TX 75390 USA.
[Kilar, Cody R.] Univ Florida, Dept Physiol & Funct Genom, Gainesville, FL 32611 USA.
[Park, Yoonjung] Univ Houston, Dept Hlth & Human Performance, Houston, TX 77204 USA.
[Narayanan, Anand] Texas A&M Univ, Dept Med Physiol, Hlth Sci Ctr, Bryan, TX 77807 USA.
[Alwood, Joshua S.; Shirazi-Fard, Yasaman; Schreurs, Ann-Sofie; Globus, Ruth K.] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
RP Delp, MD (reprint author), Florida State Univ, 120 Convocat Way, Tallahassee, FL 32306 USA.
EM mdelp@fsu.edu
OI /0000-0002-1825-7846
FU National Space and Biomedical Research Institute [MA02501]; National
Aeronautics and Space Administration (NASA) Space Biology [NNX12AL41G,
NNX14AQ57G]; NASA's Space Biology Postdoctoral Program; American Cancer
Society [RSG-14-150-01-CCE]
FX This study was supported by grants from the National Space and
Biomedical Research Institute (MA02501), National Aeronautics and Space
Administration (NASA) Space Biology (NNX12AL41G and NNX14AQ57G), the
NASA's Space Biology Postdoctoral Program (JA, AS), and the American
Cancer Society (RSG-14-150-01-CCE). We would also like to thank Luan
Tran, Betsabel Chicana and Eric Moyer for their help with the animal
husbandry and Tiffany Truong for her assistance with the bone mu CT
analysis. We thank the NASA Space Radiation Laboratory and Brookhaven
National Laboratory staff, including Peter Guida, Adam Rusek, Michael
Sivertz, Chiara La Tessa, Kristie Bonti and Laura Loudenslager for their
experimental support. Also, we thank MaryAnn Petry and the staff of
Brookhaven National Laboratory Animal Facility for their animal
husbandry support.
NR 62
TC 2
Z9 2
U1 1
U2 1
PU RADIATION RESEARCH SOC
PI LAWRENCE
PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA
SN 0033-7587
EI 1938-5404
J9 RADIAT RES
JI Radiat. Res.
PD MAR
PY 2016
VL 185
IS 3
BP 257
EP 266
DI 10.1667/RR4308.1
PG 10
WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology,
Nuclear Medicine & Medical Imaging
GA DN0KY
UT WOS:000376754000005
PM 26930379
ER
PT J
AU Sengupta, A
Cressie, N
Kahn, BH
Frey, R
AF Sengupta, Aritra
Cressie, Noel
Kahn, Brian H.
Frey, Richard
TI Predictive Inference for Big, Spatial, Non-Gaussian Data: MODIS Cloud
Data and its Change-of-Support
SO AUSTRALIAN & NEW ZEALAND JOURNAL OF STATISTICS
LA English
DT Article
DE climate projection; EM estimation; empirical Bayes; Markov Chain Monte
Carlo (MCMC); optimal spatial prediction; spatial GLMM; SRE model
ID STATISTICAL-ANALYSIS; HIERARCHICAL-MODELS; FRACTION ERRORS; TERRA;
DISTRIBUTIONS; ALGORITHM; SETS
AB Remote sensing of the earth with satellites yields datasets that can be massive in size, nonstationary in space, and non-Gaussian in distribution. To overcome computational challenges, we use the reduced-rank spatial random effects (SRE) model in a statistical analysis of cloud-mask data from NASA's Moderate Resolution Imaging Spectroradiometer (MODIS) instrument on board NASA's Terra satellite. Parameterisations of cloud processes are the biggest source of uncertainty and sensitivity in different climate models' future projections of Earth's climate. An accurate quantification of the spatial distribution of clouds, as well as a rigorously estimated pixel-scale clear-sky-probability process, is needed to establish reliable estimates of cloud-distributional changes and trends caused by climate change. Here we give a hierarchical spatial-statistical modelling approach for a very large spatial dataset of 2.75million pixels, corresponding to a granule of MODIS cloud-mask data, and we use spatial change-of-Support relationships to estimate cloud fraction at coarser resolutions. Our model is non-Gaussian; it postulates a hidden process for the clear-sky probability that makes use of the SRE model, EM-estimation, and optimal (empirical Bayes) spatial prediction of the clear-sky-probability process. Measures of prediction uncertainty are also given.
C1 [Sengupta, Aritra] Ohio State Univ, Dept Stat, Columbus, OH 43210 USA.
[Cressie, Noel] Univ Wollongong, Environm Informat Ctr, Natl Inst Appl Stat Res Australia, Sch Math & Appl Stat, Wollongong, NSW 2522, Australia.
[Kahn, Brian H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Frey, Richard] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI USA.
RP Sengupta, A (reprint author), Ohio State Univ, Dept Stat, Columbus, OH 43210 USA.
EM atrsrv@gmail.com
FU National Aeronautic and Space Administration (NASA) [NNH11ZDA001N-AIST];
NASA [NNH11ZDA001N-OCO2 (OCO-2)]; Australian Research Council
FX This research was partially supported by the National Aeronautic and
Space Administration (NASA) grant NNH11ZDA001N-AIST (Advanced
Information Systems Technology, Earth Science Technology Office) and
NASA grant NNH11ZDA001N-OCO2 (OCO-2 Science Team); and it was partially
supported by a 2015-2017 Australian Research Council Discovery Grant. We
are grateful to Amy Braverman, Mathias Schreier, and Robert Pincus for
their generous contributions to this research. We also express our
thanks to the editors and the anonymous referees for their valuable
suggestions.
NR 46
TC 0
Z9 0
U1 1
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1369-1473
EI 1467-842X
J9 AUST NZ J STAT
JI Aust. N. Z. J. Stat.
PD MAR
PY 2016
VL 58
IS 1
BP 15
EP 45
DI 10.1111/anzs.12148
PG 31
WC Statistics & Probability
SC Mathematics
GA DK1VQ
UT WOS:000374703500002
ER
PT J
AU Wilson, F
Neukirch, T
Hesse, M
Harrison, MG
Stark, CR
AF Wilson, F.
Neukirch, T.
Hesse, M.
Harrison, M. G.
Stark, C. R.
TI Particle-in-cell simulations of collisionless magnetic reconnection with
a non-uniform guide field
SO PHYSICS OF PLASMAS
LA English
DT Article
ID FORCE-FREE PLASMA; DISSIPATION REGION; CONFIGURATION
AB Results are presented of a first study of collisionless magnetic reconnection starting from a recently found exact nonlinear force-free Vlasov-Maxwell equilibrium. The initial state has a Harris sheet magnetic field profile in one direction and a non-uniform guide field in a second direction, resulting in a spatially constant magnetic field strength as well as a constant initial plasma density and plasma pressure. It is found that the reconnection process initially resembles guide field reconnection, but that a gradual transition to anti-parallel reconnection happens as the system evolves. The time evolution of a number of plasma parameters is investigated, and the results are compared with simulations starting from a Harris sheet equilibrium and a Harris sheet plus constant guide field equilibrium. (C) 2016 Author(s).
C1 [Wilson, F.; Neukirch, T.; Harrison, M. G.; Stark, C. R.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
[Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stark, C. R.] Abertay Univ, Div Comp & Math, Dundee DD1 1HG, Scotland.
RP Wilson, F; Neukirch, T (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
EM fw237@st-andrews.ac.uk; tn3@st-andrews.ac.uk
RI Stark, Craig /A-7667-2016;
OI Neukirch, Thomas/0000-0002-7597-4980
FU European Union [SHOCK 284515]; Leverhulme Trust [F/00268/BB]; U.K.
Science and Technology Facilities Council [ST/K000950/1]; NASA's
Magnetospheric Multiscale Mission; [PPA/S/S/2005/04216]
FX This project has received funding from the European Union's Seventh
Framework Programme for research, technological development, and
demonstration under Grant Agreement No. SHOCK 284515 (F.W. and T.N.).
Website: project-shock.eu/home/. We also acknowledge financial support
from the Leverhulme Trust, under Grant No. F/00268/BB (C.S., F.W., and
T.N.); the U.K. Science and Technology Facilities Council via
consolidated Grant No. ST/K000950/1 (F.W. and T.N.) and PhD studentship
Reference No. PPA/S/S/2005/04216 (M.G.H.); and NASA's Magnetospheric
Multiscale Mission (M.H.).
NR 40
TC 2
Z9 2
U1 1
U2 4
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD MAR
PY 2016
VL 23
IS 3
AR 032302
DI 10.1063/1.4942939
PG 11
WC Physics, Fluids & Plasmas
SC Physics
GA DL7XY
UT WOS:000375854900032
ER
PT J
AU Steinbock, O
Cartwright, J
Barge, L
AF Steinbock, Oliver
Cartwright, Julyan
Barge, Laura
TI The fertile physics of chemical gardens
SO PHYSICS TODAY
LA English
DT Article
ID PRECIPITATION; GENERATION
C1 [Steinbock, Oliver] Florida State Univ, Chem, Tallahassee, FL 32306 USA.
[Cartwright, Julyan] Spanish Natl Res Council, Granada, Spain.
[Barge, Laura] CALTECH, Jet Prop Lab, Planetary Chem & Astrobiol Grp, Pasadena, CA USA.
RP Steinbock, O (reprint author), Florida State Univ, Chem, Tallahassee, FL 32306 USA.
RI Cartwright, Julyan/C-1387-2016
OI Cartwright, Julyan/0000-0001-7392-0957
FU National Science Foundation [1005861, 1213259]; National Aeronautics and
Space Administration; NASA Astrobiology Institute (Icy Worlds);
[FIS2013-48444-C2-2-P]
FX Oliver Steinbock acknowledges support from the National Science
Foundation (1005861, 1213259). Julyan Cartwright received support from
Spanish project FIS2013-48444-C2-2-P. Parts of this work were carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration, with support from the NASA Astrobiology Institute (Icy
Worlds).
NR 11
TC 3
Z9 3
U1 4
U2 8
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0031-9228
EI 1945-0699
J9 PHYS TODAY
JI Phys. Today
PD MAR
PY 2016
VL 69
IS 3
BP 44
EP 51
PG 8
WC Physics, Multidisciplinary
SC Physics
GA DL7YO
UT WOS:000375856500013
ER
PT J
AU Rampe, EB
Morris, RV
Archer, PD
Agresti, DG
Ming, DW
AF Rampe, Elizabeth B.
Morris, Richard V.
Archer, P. Douglas, Jr.
Agresti, David G.
Ming, Douglas W.
TI Recognizing sulfate and phosphate complexes chemisorbed onto nanophase
weathering products on Mars using in-situ and remote observations
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Mars; nanophase minerals; chemisorption; spectroscopy; evolved gas
analysis; X-ray diffraction
ID EMISSION-SPECTROSCOPY; GALE CRATER; REFLECTANCE SPECTROSCOPY; SYNTHETIC
ALLOPHANE; MOSSBAUER DATA; VOLCANIC ASH; NEW-ZEALAND; FERRIHYDRITE;
ADSORPTION; MINERALS
AB Orbital and in-situ data from the surface of Mars indicate that nanophase weathering products are important constituents of martian rocks and soils. Nanophase minerals have the capacity to chemisorb anions like sulfate and phosphate onto their surfaces, but it is not known whether chemisorption is an important or even detectable process via orbital and in-situ observations. The detection of chemisorbed sulfate and phosphate anions on nanophase minerals would constrain the speciation of these anions and past aqueous environmental conditions. Here, we synthesized two nanophase weathering products that are common in terrestrial volcanic soils and have been identified on the martian surface: allophane and nanophase ferric oxide as represented by ferrihydrite. We specifically adsorbed sulfate and phosphate separately onto the nanophase mineral surfaces (4.5 and 1.6 wt% SO42-, and 6.7 and 8.9 wt% PO43- on allophane and ferrihydrite, respectively) and analyzed the untreated and chemisorbed materials using instruments similar to those on orbital and landed Mars missions (including X-ray diffraction, evolved gas analysis, Mossbauer spectroscopy, and VNIR and thermal-IR spectroscopy). Evolved gas analysis is the optimum method to detect chemisorbed sulfate, with SO2(g) being released at >900 degrees C for allophane and 400-800 degrees C for ferrihydrite. Chemisorbed sulfate and phosphate anions affect the thermal-IR spectra of allophane and ferrihydrite in the S-O and P-O stretching region when present in abundances of only a few weight percent; S-O and P-O stretching bands are apparent as short-wavelength shoulders on Si-O stretching bands. Sulfate and phosphate anions chemisorbed to allophane have small but measurable effects on the position of the OH-H2O bands at 1.4 and 1.9 mu m in near-IR spectra. Chemisorbed sulfate and phosphate anions did not affect the X-ray diffraction patterns, Mossbauer spectra, and visible/near-IR spectra of ferrihydrite. These data suggest that sulfate chemisorbed onto the surfaces of nanophase minerals can be detected with the Sample Analysis at Mars (SAM) instrument on the Mars science laboratory Curiosity rover, and subtle signatures of chemisorbed sulfate and phosphate may be detectable by IR spectrometers on landed missions. The combined use of SAM, the Chemistry and Mineralogy (CheMin) instrument, and the Alpha Particle X-ray Spectrometer (APXS) on Curiosity allows for the most detailed characterization to date of nanophase minerals in martian rocks and soils and the potential presence of chemisorbed anionic complexes.
C1 [Rampe, Elizabeth B.] NASA, Aerodyne Ind, Jacobs JETS Contract, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mail Code XI3, Houston, TX 77058 USA.
[Morris, Richard V.; Ming, Douglas W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Archer, P. Douglas, Jr.] NASA, Jacobs, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Agresti, David G.] Univ Alabama Birmingham, Dept Phys, Birmingham, AL 35294 USA.
RP Rampe, EB (reprint author), NASA, Aerodyne Ind, Jacobs JETS Contract, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mail Code XI3, Houston, TX 77058 USA.
EM elizabeth.b.rampe@nasa.gov
FU NASA Mars Fundamental Research Program
FX We gratefully acknowledge the Mars Space Flight Facility at Arizona
State University for the use of their Thermal-IR spectroscopy
laboratory; Alicia Rutledge for her help measuring TIR spectra; Charlie
Galindo, Dean Muir, and Chris Carrier for measuring IC data; Roy
Christofferson for TEM analyses; DC Golden for his expert advice on
nanophase mineral syntheses and ion adsorption procedures; and Janice
Bishop, Enver Murad, and an anonymous reviewer for their constructive
comments on the manuscript. This work was funded by the NASA Mars
Fundamental Research Program in an award to E.B. Rampe and R.V. Morris.
NR 80
TC 1
Z9 1
U1 7
U2 12
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD MAR-APR
PY 2016
VL 101
IS 3-4
BP 678
EP 689
DI 10.2138/am-2016-5408CCBYNCND
PG 12
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA DK0TW
UT WOS:000374626100014
ER
PT J
AU Cai, CX
Kulkarni, S
Zhao, Z
Kaduwela, AP
Avise, JC
DaMassa, JA
Singh, HB
Weinheimer, AJ
Cohen, RC
Diskin, GS
Wennberg, P
Dibb, JE
Huey, G
Wisthaler, A
Jimenez, JL
Cubison, MJ
AF Cai, Chenxia
Kulkarni, Sarika
Zhao, Zhan
Kaduwela, Ajith P.
Avise, Jeremy C.
DaMassa, John A.
Singh, Hanwant B.
Weinheimer, Andrew J.
Cohen, Ronald C.
Diskin, Glenn S.
Wennberg, Paul
Dibb, Jack E.
Huey, Greg
Wisthaler, Armin
Jimenez, Jose L.
Cubison, Michael J.
TI Simulating reactive nitrogen, carbon monoxide, and ozone in California
during ARCTAS-CARB 2008 with high wildfire activity
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Ozone; Carbon monoxide; Reactive nitrogen; San Joaquin valley; South
coast air basin; Wildfires
ID SAN-JOAQUIN VALLEY; LOS-ANGELES BASIN; AIR-QUALITY;
SATELLITE-OBSERVATIONS; FIRE EMISSIONS; VOC REACTIVITY; SILAGE GAS;
MODEL; POLLUTION; NOX
AB Predictions of O-3, CO, total NOy and individual NOy species (NO, NO2, HNO3, PAN, alkyl nitrates and aerosol nitrate) from a fine resolution regional air quality modeling system for the South Coast Air Basin (SoCAB) and San Joaquin Valley Air Basin (SJVAB) of California are presented and evaluated for the 2008 ARCTAS-CARB campaign. The measurements of the chemical compounds from the fire plumes during the field campaign allow for the evaluation of the model's ability to simulate fire-influenced air masses as well. In general, the model successfully simulated the broad spatial distribution of chemical compounds in both air basins as well as the variation within the basins. Using inventories that reflect 2008 emissions levels, the model performed well in simulating NOx (NO + NO2) in SoCAB. Therefore, the under prediction of O-3 over these areas is more likely caused by uncertainties with the VOC emissions, chemistry, or discrepancies in the meteorology. The model did not capture the relatively high levels of O-3, and some reactive nitrogen species that were measured off shore of the SoCAB, indicating potential missing sources or the transport from on shore to off shore was not successfully captured. In SJVAB, the model had good performance in simulating different chemical compounds in the Fresno and Arvin areas. However, enhanced concentrations of O-3, NOx, HNO3 and PAN near dairy farms were significantly underestimated in the model. Negative biases also exist for O-3 and HNO3 near oil fields, suggesting larger uncertainties associated with these emission sources. While the model simulated the total NOy mixing ratios reasonably well, the prediction for partitioning between individual compounds showed larger uncertainties in the model simulation. Although the fire emissions inventory was updated to include the latest emissions estimates and speciation profiles, our model shows limited improvement in simulating the enhancement of O-3, CO, and PAN under fire impact as compared to a previous version of the modeling system. Further improvements in simulating fire emissions, especially the timing and the plume injection heights, are desired in order to better simulate the impact of fires. Published by Elsevier Ltd.
C1 [Cai, Chenxia; Kulkarni, Sarika; Zhao, Zhan; Kaduwela, Ajith P.; Avise, Jeremy C.; DaMassa, John A.] Calif Air Resources Board, Air Qual Planning & Sci Div, Sacramento, CA 95814 USA.
[Kaduwela, Ajith P.] Univ Calif Davis, Air Qual Res Ctr, Davis, CA 95616 USA.
[Avise, Jeremy C.] Washington State Univ, Dept Civil & Environm Engn, Pullman, WA 99164 USA.
[Singh, Hanwant B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Weinheimer, Andrew J.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Cohen, Ronald C.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
[Cohen, Ronald C.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Diskin, Glenn S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Wennberg, Paul] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
[Wennberg, Paul] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Dibb, Jack E.] Univ New Hampshire, Inst Study Earth Ocean & Space, Earth Syst Res Ctr, Durham, NH 03824 USA.
[Huey, Greg] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Wisthaler, Armin] Univ Innsbruck, Inst Ion Phys & Appl Phys, A-6020 Innsbruck, Austria.
[Jimenez, Jose L.] Univ Colorado, Dept Chem, Boulder, CO 80309 USA.
[Jimenez, Jose L.; Cubison, Michael J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
RP Cai, CX (reprint author), Calif Air Resources Board, Air Qual Planning & Sci Div, Sacramento, CA 95814 USA.
EM Chenxia.Cai@arb.ca.gov
RI Cohen, Ronald/A-8842-2011; Jimenez, Jose/A-5294-2008;
OI Cohen, Ronald/0000-0001-6617-7691; Jimenez, Jose/0000-0001-6203-1847;
Kaduwela, Ajith/0000-0002-7236-2698
FU NASA Tropospheric Chemistry Program; NASA Radiation Sciences Program;
California Air Resources Board
FX The ARCTAS-CARB campaign was funded by the NASA Tropospheric Chemistry
Program, the NASA Radiation Sciences Program, and the California Air
Resources Board. CH3CN measurements were supported by the
Austrian Federal Ministry for Transport, Innovation and Technology
through the Austrian Space Applications Programme of the Austrian
Research Promotion Agency. Tomas Mikoviny is acknowledged for his
contribution in the CH3CN data analysis. We thank all
ARCTAS-CARB participants for their support and contributions. Vernon
Hughes at CARB provided us with the emissions inventories used in this
study. We also thank Eileen McCauley, Dazhong Yin, Bruce Jackson, Jin
Lu, Adam Gerber and Klaus Scott of CARB for valuable discussions.
NR 84
TC 3
Z9 3
U1 13
U2 27
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD MAR
PY 2016
VL 128
BP 28
EP 44
DI 10.1016/j.atmosenv.2015.12.031
PG 17
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DL6EH
UT WOS:000375731900004
ER
PT J
AU Gkikas, A
Hatzianastassiou, N
Mihalopoulos, N
Torres, O
AF Gkikas, A.
Hatzianastassiou, N.
Mihalopoulos, N.
Torres, O.
TI Characterization of aerosol episodes in the greater Mediterranean Sea
area from satellite observations (2000-2007)
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Aerosol episodes; Aerosol type; Dust; Sea-salt; Frequency; Intensity;
Satellites; Mediterranean
ID LONG-RANGE TRANSPORT; DESERT-DUST EPISODES; OPTICAL-PROPERTIES; SAHARAN
DUST; RAMAN LIDAR; MODIS DATA; SEASONAL VARIABILITY;
CHEMICAL-COMPOSITION; GLOBAL DISTRIBUTION; ARABIAN PENINSULA
AB An algorithm able to identify and characterize episodes of different aerosol types above sea surfaces of the greater Mediterranean basin (GMB), including the Black Sea and the Atlantic Ocean off the coasts of Iberia and northwest Africa, is presented in this study. Based on this algorithm, five types of intense (strong and extreme) aerosol episodes in the GMB are identified and characterized using daily aerosol optical properties from satellite measurements, namely MODIS-Terra, Earth Probe (EP)-TOMS and OMI-Aura. These aerosol episodes are: (i) biomass-burning/urban-industrial (BU), (ii) desert dust (DD), (iii) dust/sea-salt (DSS), (iv) mixed (MX) and (v) undetermined (UN). The identification and characterization is made with our algorithm using a variety of aerosol properties, namely aerosol optical depth (AOD), Angstrom exponent (a), fine fraction (FF), effective radius (r(eff)) and Aerosol Index (AI).
During the study period (2000-2007), the most frequent aerosol episodes are DD, observed primarily in the western and central Mediterranean Sea, and off the northern African coasts, 7 times/year for strong episodes and 4 times/year for extreme ones, on average. The DD episodes yield 40% of all types of strong aerosol episodes in the study region, while they account for 71.5% of all extreme episodes. The frequency of occurrence of strong episodes exhibits specific geographical patterns, for example the BU are mostly observed along the coasts of southern Europe and off the Atlantic coasts of Portugal, the MX episodes off the Spanish Mediterranean coast and over the Adriatic and northern Aegean Sea, while the DSS ones over the western and central Mediterranean Sea. On the other hand, the extreme episodes for all but DD aerosol display more patchy spatial patterns. The strong episodes exhibit AOD at 550 nm as high as 1.6 in the southernmost parts of central and eastern Mediterranean Sea, which rise up to 5 for the extreme, mainly DD and DSS, episodes. Although more than 90% of all aerosol episodes last I day, there are few cases, mainly extreme DD episodes, which last up to 4 days. Independently of their type, the Mediterranean aerosol episodes occur more frequently in spring (strong and extreme episodes) and summer (strong episodes) and most rarely during winter. A significant year by year variability of Mediterranean aerosol episodes has been identified, more in terms of their frequency than intensity. An analysis of 5-day back trajectories for the most extreme episodes provides confidence on the obtained results of the algorithm, based on the revealed origin and track of air masses causing the episodes. The 25 and 6% of all strong and extreme episodes, respectively, are MX, thus highlighting the co-existence of different aerosol types in the greater Mediterranean. The intensity of both MX and DSS episodes exhibits similar patterns to those of DD strong ones, indicating that desert dust is a determinant factor for the intensity of aerosol episodes in the Mediterranean, including DSS and MX episodes. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Gkikas, A.; Hatzianastassiou, N.] Univ Ioannina, Lab Meteorol, Dept Phys, GR-45110 Ioannina, Greece.
[Gkikas, A.] Barcelona Supercomp Ctr, Dept Earth Sci, Barcelona, Spain.
[Mihalopoulos, N.] Univ Crete, Environm Chem Proc Lab, Dept Chem, Iraklion, Greece.
[Mihalopoulos, N.] NOA, Inst Environm Res & Sustainable Dev, Athens, Greece.
[Torres, O.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
RP Hatzianastassiou, N (reprint author), Univ Ioannina, Lab Meteorol, Dept Phys, GR-45110 Ioannina, Greece.
EM nhatzian@cc.uol.gr
RI GKIKAS, ANTONIS/F-4184-2017; Mihalopoulos, Nikolaos/H-5327-2016
OI GKIKAS, ANTONIS/0000-0002-4137-0724; Mihalopoulos,
Nikolaos/0000-0002-1282-0896
FU European Union (European Social Fund - ESF); Greek national funds
through the operational programme "Education and Lifelong Learning" of
the National Strategic Reference Framework (NSRF) - Research Funding
Program: ARISTEIA-PANOPLY Investing in knowledge society through the
European Social Fund
FX The Earth Probe (TOMS) and OMI aerosol climatology is available from the
TOMS Web site (http://toms.gsfc.nasa.gov). The Collection 005 MODIS
Terra data were obtained from NASA's MODIS Data Processing System
(MODAPS) website (ftp://ladsweb.nascom.nasa.gov/). The authors
gratefully acknowledge the NOAA Air Resources Laboratory (ARL) for the
provision of the HYSPLIT transport and dispersion model and/or READY
website (http://ready.arl.noaa.gov) used in this publication. NH and NM
acknowledge support by the European Union (European Social Fund - ESF)
and Greek national funds through the operational programme "Education
and Lifelong Learning" of the National Strategic Reference Framework
(NSRF) - Research Funding Program: ARISTEIA-PANOPLY Investing in
knowledge society through the European Social Fund.
NR 110
TC 5
Z9 5
U1 3
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD MAR
PY 2016
VL 128
BP 286
EP 304
DI 10.1016/j.atmosenv.2015.11.056
PG 19
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DL6EH
UT WOS:000375731900028
ER
PT J
AU Wilson, C
Gloor, M
Gatti, LV
Miller, JB
Monks, SA
McNorton, J
Bloom, AA
Basso, LS
Chipperfield, MP
AF Wilson, Chris
Gloor, Manuel
Gatti, Luciana V.
Miller, John B.
Monks, Sarah A.
McNorton, Joey
Bloom, A. Anthony
Basso, Luana S.
Chipperfield, Martyn P.
TI Contribution of regional sources to atmospheric methane over the Amazon
Basin in 2010 and 2011
SO GLOBAL BIOGEOCHEMICAL CYCLES
LA English
DT Article
ID CHEMICAL-TRANSPORT MODEL; BIOMASS BURNING EMISSIONS; ASSIMILATION
SYSTEM; LOWER STRATOSPHERE; NATURAL WETLANDS; GROWTH-RATE; VARIABILITY;
FLUX; DEFORESTATION; GASES
AB We present an assessment of methane (CH4) atmospheric concentrations over the Amazon Basin for 2010 and 2011 using a 3-D atmospheric chemical transport model, two wetland emission models, and new observations made during biweekly flights made over four locations within the basin. We attempt to constrain basin-wide CH4 emissions using the observations, and since 2010 was an unusually dry year, we assess the effect of this drought on Amazonian methane emissions. We find that South American emissions contribute up to 150 ppb to concentrations at the sites, mainly originating from within the basin. Our atmospheric model simulations agree reasonably well with measurements at three of the locations (0.28 <= r(2) <= 0.63, mean bias <= 9.5 ppb). Attempts to improve the simulated background CH4 concentration through analysis of simulated and observed sulphur hexafluoride concentrations do not improve the model performance, however. Through minimisation of seasonal biases between the simulated and observed atmospheric concentrations, we scale our prior emission inventories to derive total basin-wide methane emissions of 36.5-41.1 Tg(CH4)/yr in 2010 and 31.6-38.8 Tg(CH4)/yr in 2011. These totals suggest that the Amazon contributes significantly (up to 7%) to global CH4 emissions. Our analysis indicates that factors other than precipitation, such as temperature variations or tree mortality, may have affected microbial emission rates. However, given the uncertainty of our emission estimates, we cannot say definitively whether the noncombustion emissions from the region were different in 2010 and 2011, despite contrasting meteorological conditions between the two years.
C1 [Wilson, Chris; McNorton, Joey; Chipperfield, Martyn P.] Univ Leeds, Natl Ctr Earth Observat, Leeds, W Yorkshire, England.
[Wilson, Chris; Monks, Sarah A.; McNorton, Joey; Chipperfield, Martyn P.] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England.
[Wilson, Chris; Gloor, Manuel] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
[Gatti, Luciana V.; Basso, Luana S.] Comissao Nacl Energia Nucl, Inst Pesquisas Energet & Nucl, Atmospher Chem Lab, Sao Paulo, Brazil.
[Miller, John B.] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO USA.
[Miller, John B.; Monks, Sarah A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Monks, Sarah A.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO USA.
[Bloom, A. Anthony] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Wilson, C (reprint author), Univ Leeds, Natl Ctr Earth Observat, Leeds, W Yorkshire, England.; Wilson, C (reprint author), Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England.; Wilson, C (reprint author), Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
EM c.wilson@leeds.ac.uk
RI Chipperfield, Martyn/H-6359-2013; Gatti, Luciana/J-8569-2012;
OI Chipperfield, Martyn/0000-0002-6803-4149; MONKS,
SARAH/0000-0003-3474-027X; Wilson, Chris/0000-0001-8494-0697
FU UK Natural Environment Research Council (NERC); National Centre for
Earth Observation (NCEO); NERC Consortiumgrants for AMAZONICA
[NE/F005806/1]; Amazon hydrological cycle [NE/K01353X/1]; EU 7th
Framework GEOCARBON project grant [283080]; CNPq; FAPESP; CIRES;
NOAA/ESRL; CAPES; NOAA Climate Program Office's Atmospheric Chemistry,
Carbon Cycle, and Climate (AC4) program; Royal Society Wolfson Merit
Award
FX CH4, CO, and SF6 vertical profile observations
made as part of the AMAZONICA project will be made available through the
World Meteorological Organisation's repository, the World Data Center
for Greenhouse Gases (http://ds.data.jma.go.jp/gmd/wdcgg/) soon after
publication of this manuscript. This work was supported by the UK
Natural Environment Research Council (NERC) and the National Centre for
Earth Observation (NCEO). Financial support was from the NERC
Consortiumgrants for AMAZONICA (NE/F005806/1) and the Amazon
hydrological cycle (NE/K01353X/1), along with the EU 7th Framework
GEOCARBON project grant (grant agreement 283080), CNPq and FAPESP. M.G.
also acknowledges a bolsa from the Brazilian ciencia sem fronteiras
program and a visiting fellowship at CIRES and NOAA/ESRL, and LG support
from CNPq, CAPES, and FAPESP. J.B.M. thanks the NOAA Climate Program
Office's Atmospheric Chemistry, Carbon Cycle, and Climate (AC4) program
for support, including that for collection and analysis of NOAA
CH4 observations used in this study. MPC is partly funded by
a Royal Society Wolfson Merit Award. The TOMCAT simulations were run on
the UK National Supercomputing Service ARCHER and University of Leeds
ARC2 computing facilities. We thankWuhu Feng (NCAS) for help with the
TOMCAT model and Andrew Crotwell (NOAA) for instrument development.
NR 78
TC 3
Z9 3
U1 5
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0886-6236
EI 1944-9224
J9 GLOBAL BIOGEOCHEM CY
JI Glob. Biogeochem. Cycle
PD MAR
PY 2016
VL 30
IS 3
BP 400
EP 420
DI 10.1002/2015GB005300
PG 21
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA DJ8QO
UT WOS:000374477400001
ER
PT J
AU Schmidt, JM
Cairns, IH
Xie, H
Cyr, OCS
Gopalswamy, N
AF Schmidt, J. M.
Cairns, Iver H.
Xie, Hong
Cyr, O. C. St.
Gopalswamy, N.
TI CME flux rope and shock identifications and locations: Comparison of
white light data, Graduated Cylindrical Shell model, and MHD simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CORONAL MASS EJECTION; RADIO-EMISSION SIMULATIONS; MAGNETOHYDRODYNAMIC
MODEL; FILAMENT ERUPTIONS; LASCO OBSERVATIONS; DRIVEN SHOCKS;
LARGE-ANGLE; SOLAR-WIND; ACCELERATION; PREDICTION
AB Coronal mass ejections (CMEs) are major transient phenomena in the solar corona that are observed with ground-based and spacecraft-based coronagraphs in white light or with in situ measurements by spacecraft. CMEs transport mass and momentum and often drive shocks. In order to derive the CME and shock trajectories with high precision, we apply the graduated cylindrical shell (GCS) model to fit a flux rope to the CME directed toward STEREO A after about 19:00 UT on 29 November 2013 and check the quality of the heliocentric distance-time evaluations by carrying out a three-dimensional magnetohydrodynamic (MHD) simulation of the same CME with the Block Adaptive Tree Solar-Wind Roe Upwind Scheme (BATS-R-US) code. Heliocentric distances of the CME and shock leading edges are determined from the simulated white light images and magnetic field strength data. We find very good agreement between the predicted and observed heliocentric distances, showing that the GCS model and the BATS-R-US simulation approach work very well and are consistent. In order to assess the validity of CME and shock identification criteria in coronagraph images, we also compute synthetic white light images of the CME and shock. We find that the outer edge of a cloud-like illuminated area in the observed and predicted images in fact coincides with the leading edge of the CME flux rope and that the outer edge of a faint illuminated band in front of the CME leading edge coincides with the CME-driven shock front.
C1 [Schmidt, J. M.; Cairns, Iver H.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
[Xie, Hong; Cyr, O. C. St.; Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Xie, Hong] Catholic Univ Amer, Washington, DC 20064 USA.
RP Schmidt, JM (reprint author), Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
EM jschmidt@physics.usyd.edu.au
OI Schmidt, Joachim/0000-0002-7927-0665; Cairns, Iver/0000-0001-6978-9765
FU Australian Research Council [DP140103933]; NASA LWS grant [NNX15AB70G];
NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI
FX We gratefully acknowledge funding via grant DP140103933 from the
Australian Research Council. Hong Xie was supported by NASA LWS grant
number NNX15AB70G. The CME simulations were carried out using the Space
Weather Modeling Framework, a development of the Center for Space
Environment Modeling at the University of Michigan that was funded by
NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. CME data are taken from
the CDAW list at NASA. All data for this paper are cited and referred to
in the reference list.
NR 48
TC 1
Z9 1
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2016
VL 121
IS 3
BP 1886
EP 1906
DI 10.1002/2015JA021805
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DK2FV
UT WOS:000374730900005
ER
PT J
AU Randol, BM
Christian, ER
AF Randol, Brent M.
Christian, Eric R.
TI Coupling of charged particles via Coulombic interactions: Numerical
simulations and resultant kappa-like velocity space distribution
functions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID COMPUTER-SIMULATION; SUPRATHERMAL TAILS; SOLAR-WIND; ACCELERATION;
HELIOSPHERE; SPECTRA; EQUILIBRIUM; PLASMAS
AB A parametric study is performed using the electrostatic simulations of Randol and Christian (2014) in which the number density, n, and initial thermal speed, theta, are varied. The range of parameters covers an extremely broad plasma regime, all the way from the very weak coupling of space plasmas to the very strong coupling of solid plasmas. The first result is that simulations at the same Gamma(D), where Gamma(D) (alpha n(1/3) theta(-2)) is the plasma coupling parameter, but at different combinations of n and theta, behave exactly the same. As a function of Gamma(D), the form of p(v), the velocity distribution function of v, the magnitude of v, the velocity vector, is studied. For intermediate to high Gamma(D), heating is observed in p(v) that obeys conservation of energy, and a suprathermal tail is formed, with a spectral index that depends on GD. For strong coupling (Gamma(D) >> 1), the form of the tail is v(-5), consistent with the findings of Randol and Christian (2014). For weak coupling (Gamma(D) << 1), no acceleration or heating occurs, as there is no free energy. The dependence on N, the number of particles in the simulation, is also explored. There is a subtle dependence in the index of the tail, such that v(-5) appears to be the N -> infinity limit.
C1 [Randol, Brent M.; Christian, Eric R.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.
[Randol, Brent M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Randol, BM (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.; Randol, BM (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM brent.m.randol@nasa.edu
NR 23
TC 0
Z9 0
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2016
VL 121
IS 3
BP 1907
EP 1919
DI 10.1002/2015JA021859
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DK2FV
UT WOS:000374730900006
ER
PT J
AU Selesnick, RS
Baker, DN
Jaynes, AN
Li, X
Kanekal, SG
Hudson, MK
Kress, BT
AF Selesnick, R. S.
Baker, D. N.
Jaynes, A. N.
Li, X.
Kanekal, S. G.
Hudson, M. K.
Kress, B. T.
TI Inward diffusion and loss of radiation belt protons
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CRRES OBSERVATIONS; ENERGY; WAVES
AB Radiation belt protons in the kinetic energy range 24 to 76 MeV are being measured by the Relativistic Electron Proton Telescope on each of the two Van Allen Probes. Data have been processed for the purpose of studying variability in the trapped proton intensity during October 2013 to August 2015. For the lower energies (less than or similar to 32 MeV), equatorial proton intensity near L = 2 showed a steady increase that is consistent with inward diffusion of trapped solar protons, as shown by positive radial gradients in phase space density at fixed values of the first two adiabatic invariants. It is postulated that these protons were trapped with enhanced efficiency during the 7 March 2012 solar proton event. A model that includes radial diffusion, along with known trapped proton source and loss processes, shows that the observed average rate of increase near L = 2 is predicted by the same model diffusion coefficient that is required to form the entire proton radiation belt, down to low L, over an extended (similar to 10(3) year) interval. A slower intensity decrease for lower energies near L = 1.5 may also be caused by inward diffusion, though it is faster than predicted by the model. Higher-energy (greater than or similar to 40 MeV) protons near the L = 1.5 intensity maximum are from cosmic ray albedo neutron decay. Their observed intensity is lower than expected by a factor similar to 2, but the discrepancy is resolved by adding an unspecified loss process to the model with a mean lifetime similar to 120 years.
C1 [Selesnick, R. S.] US Air Force, Res Lab, Space Vehicles Directorate, Kirtland AFB, NM USA.
[Baker, D. N.; Jaynes, A. N.; Li, X.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Li, X.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
[Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Hudson, M. K.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Kress, B. T.] Univ Colorado, Ctr Cooperat Res Environm Sci, Boulder, CO 80309 USA.
[Kress, B. T.] NOAA, Natl Ctr Environm Informat, Boulder, CO USA.
RP Selesnick, RS (reprint author), US Air Force, Res Lab, Space Vehicles Directorate, Kirtland AFB, NM USA.
EM richard.selesnick@us.af.mil
FU NASA [NNH14AX18I]; Air Force Research Laboratory under the Heliophysics
Guest Investigators Program, at University of Colorado and Dartmouth
College by RBSP-ECT through JHU/APL contract under prime NASA [967399,
NAS5-01072]; Air Force Research Laboratory under the Heliophysics Guest
Investigators Program, Dartmouth College, by NASA grant [NNX15AF54G];
National Science Foundation [AGS-1455470]
FX Van Allen Probes REPT and ephemeris data are available from the ECT
Science Operations and Data Center, http://www.rbsp-ect.lanl.gov;
EMFISIS data are available from http://emfisis.physics.uiowa.edu. We
thank T.P. O'Brien for pointing out the work of Schulz [1975]. This work
was supported in part by NASA agreement NNH14AX18I with the Air Force
Research Laboratory under the Heliophysics Guest Investigators Program,
at University of Colorado and Dartmouth College by RBSP-ECT funding
through JHU/APL contract 967399 under prime NASA contract NAS5-01072,
and, at Dartmouth College, by NASA grant NNX15AF54G and National Science
Foundation grant AGS-1455470.
NR 23
TC 3
Z9 3
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2016
VL 121
IS 3
BP 1969
EP 1978
DI 10.1002/2015JA022154
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DK2FV
UT WOS:000374730900011
ER
PT J
AU Sigsbee, K
Kletzing, CA
Smith, CW
MacDowall, R
Spence, H
Reeves, G
Blake, JB
Baker, DN
Green, JC
Singer, HJ
Carr, C
Santolik, O
AF Sigsbee, K.
Kletzing, C. A.
Smith, C. W.
MacDowall, R.
Spence, H.
Reeves, G.
Blake, J. B.
Baker, D. N.
Green, J. C.
Singer, H. J.
Carr, C.
Santolik, O.
TI Van Allen Probes, THEMIS, GOES, and Cluster observations of EMIC waves,
ULF pulsations, and an electron flux dropout
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ION-CYCLOTRON WAVES; RADIATION BELT ELECTRONS; 1-2 MAGNETIC PULSATIONS;
RING CURRENT; EQUATORIAL MAGNETOSPHERE; RELATIVISTIC ELECTRONS;
PLASMASPHERIC PLUME; GEOMAGNETIC STORMS; SYNCHRONOUS ORBIT; MAGNETOPAUSE
AB We examined an electron flux dropout during the 12-14 November 2012 geomagnetic storm using observations from seven spacecraft: the two Van Allen Probes, Time History of Events and Macroscale Interactions during Substorms (THEMIS)-A (P5), Cluster 2, and Geostationary Operational Environmental Satellites (GOES) 13, 14, and 15. The electron fluxes for energies greater than 2.0 MeV observed by GOES 13, 14, and 15 at geosynchronous orbit and by the Van Allen Probes remained at or near instrumental background levels for more than 24 h from 12 to 14 November. For energies of 0.8 MeV, the GOES satellites observed two shorter intervals of reduced electron fluxes. The first interval of reduced 0.8 MeV electron fluxes on 12-13 November was associated with an interplanetary shock and a sudden impulse. Cluster, THEMIS, and GOES observed intense He+ electromagnetic ion cyclotron (EMIC) waves from just inside geosynchronous orbit out to the magnetopause across the dayside to the dusk flank. The second interval of reduced 0.8 MeV electron fluxes on 13-14 November was associated with a solar sector boundary crossing and development of a geomagnetic storm with Dst <- 100nT. At the start of the recovery phase, both the 0.8 and 2.0 MeV electron fluxes finally returned to near prestorm values, possibly in response to strong ultralow frequency (ULF) waves observed by the Van Allen Probes near dawn. A combination of adiabatic effects, losses to the magnetopause, scattering by EMIC waves, and acceleration by ULF waves can explain the observed electron behavior.
C1 [Sigsbee, K.; Kletzing, C. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Smith, C. W.; Spence, H.] Univ New Hampshire, Inst Earth Oceans & Space, Durham, NH 03824 USA.
[MacDowall, R.] NASA, Goddard Space Flight Ctr, Planetary Magnetospheres Lab, Greenbelt, MD USA.
[Reeves, G.] Los Alamos Natl Lab, Space & Atmospher Sci, NIS 1, Los Alamos, NM USA.
[Blake, J. B.] Aerosp Corp, El Segundo, CA 90245 USA.
[Baker, D. N.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Green, J. C.] Space Hazards Applicat, Golden, CO USA.
[Singer, H. J.] NOAA, Space Weather Predict Ctr, Boulder, CO USA.
[Carr, C.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London, England.
[Santolik, O.] Inst Atmospher Phys AS CR, Prague, Czech Republic.
[Santolik, O.] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic.
RP Sigsbee, K (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
EM kristine-sigsbee@uiowa.edu
RI Santolik, Ondrej/F-7766-2014;
OI Kletzing, Craig/0000-0002-4136-3348; Sigsbee,
Kristine/0000-0001-8727-380X; Reeves, Geoffrey/0000-0002-7985-8098
FU JHU/APL under NASA prime contract [921647, 967399, NAS5-01072]; Czech
Academy of Sciences through the Praemium Academiae award; NASA
[NAS5-02099]; German Ministry for Economy and Technology; German Center
for Aviation and Space (DLR) [50 OC 0302]; [LH14010]
FX This work was performed under JHU/APL contract 921647 under NASA prime
contract NAS5-01072. We acknowledge William Kurth for providing density
calculations from the EMFISIS data. RBSP-ECT funding was provided by
JHU/APL contract 967399 under NASA prime contract NAS5-01072. O.
Santolik acknowledges funding from the Czech Academy of Sciences through
the Praemium Academiae award and from the LH14010 grant. We acknowledge
NASA contract NAS5-02099 and V. Angelopoulos for use of data from the
THEMIS Mission. Specifically, K.H. Glassmeier, U. Auster, and W.
Baumjohann provided THEMIS FGM data under the lead of the Technical
University of Braunschweig and with financial support through the German
Ministry for Economy and Technology and the German Center for Aviation
and Space (DLR) under contract 50 OC 0302. Data from the Van Allen
Probes can be obtained through the Van Allen Probes Science Gateway
(http://rbspgway.jhuapl.edu/). GOES data are available from the NOAA
National Geophysical Data Center, and the Preliminary Reports and
Forecasts of Solar Geophysical Data are available from the NOAA Space
Weather Prediction Center. THEMIS data are publicly available through
the University of California Berkeley (http://themis.ssl.berkeley.edu).
Cluster data are available from the Cluster Science Archive. Solar wind
data and geomagnetic indexes are available online from NASA OMNIWeb.
Wind and ACE data are available online through CDAWeb.
NR 62
TC 1
Z9 1
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2016
VL 121
IS 3
BP 1990
EP 2008
DI 10.1002/2014JA020877
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DK2FV
UT WOS:000374730900013
ER
PT J
AU Mackler, DA
Jahn, JM
Perez, JD
Pollock, CJ
Valek, PW
AF Mackler, D. A.
Jahn, J. -M.
Perez, J. D.
Pollock, C. J.
Valek, P. W.
TI Statistical correlation of low-altitude ENA emissions with geomagnetic
activity from IMAGE/MENA observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID AURORAL PROTON PRECIPITATION; TIME RING CURRENT; MAGNETIC STORM;
EQUATORWARD BOUNDARY; SCANNING PHOTOMETER; ION PRECIPITATION;
FAR-ULTRAVIOLET; DIFFUSE AURORA; MISSION; IMAGER
AB Plasma sheet particles transported Earthward during times of active magnetospheric convection can interact with exospheric/thermospheric neutrals through charge exchange. The resulting Energetic Neutral Atoms (ENAs) are free to leave the influence of the magnetosphere and can be remotely detected. ENAs associated with low-altitude (300-800km) ion precipitation in the high-latitude atmosphere/ionosphere are termed low-altitude emissions (LAEs). Remotely observed LAEs are highly nonisotropic in velocity space such that the pitch angle distribution at the time of charge exchange is near 90 degrees. The Geomagnetic Emission Cone of LAEs can be mapped spatially, showing where proton energy is deposited during times of varying geomagnetic activity. In this study we present a statistical look at the correlation between LAE flux (intensity and location) and geomagnetic activity. The LAE data are from the MENA imager on the IMAGE satellite over the declining phase of solar cycle 23 (2000-2005). The SYM-H, AE, and Kp indices are used to describe geomagnetic activity. The goal of the study is to evaluate properties of LAEs in ENA images and determine if those images can be used to infer properties of ion precipitation. Results indicate a general positive correlation to LAE flux for all three indices, with the SYM-H showing the greatest sensitivity. The magnetic local time distribution of LAEs is centered about midnight and spreads with increasing activity. The invariant latitude for all indices has a slightly negative correlation. The combined results indicate LAE behavior similar to that of ion precipitation.
C1 [Mackler, D. A.; Jahn, J. -M.; Valek, P. W.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA.
[Mackler, D. A.; Jahn, J. -M.; Valek, P. W.] Southwest Res Inst, San Antonio, TX USA.
[Perez, J. D.] Auburn Univ, Dept Phys, Auburn, AL 36849 USA.
[Pollock, C. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Mackler, DA (reprint author), Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA.; Mackler, DA (reprint author), Southwest Res Inst, San Antonio, TX USA.
EM mackler.david@gmail.com
OI Valek, Philip/0000-0002-2318-8750
FU NASA grant [NNX10-AL21G]
FX We are thankful for the many talented people at SwRI for their wisdom.
This work was supported at SwRI under NASA grant NNX10-AL21G. IMAGE MENA
data can be found at http://guinan.space.swri.edu/IMAGE/.
NR 67
TC 0
Z9 0
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2016
VL 121
IS 3
BP 2046
EP 2066
DI 10.1002/2015JA021545
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DK2FV
UT WOS:000374730900016
ER
PT J
AU Wang, S
Chen, LJ
Bessho, N
Kistler, LM
Shuster, JR
Guo, RL
AF Wang, Shan
Chen, Li-Jen
Bessho, Naoki
Kistler, Lynn M.
Shuster, Jason R.
Guo, Ruilong
TI Electron heating in the exhaust of magnetic reconnection with negligible
guide field
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID GEOTAIL OBSERVATIONS; DIFFUSION REGION; ACCELERATION; MAGNETOTAIL;
REVERSALS; SUBSTORM; DYNAMICS; PARALLEL; ION
AB Electron heating in the magnetic reconnection exhaust is investigated with particle-in-cell simulations, space observations, and theoretical analysis. Spatial variations of the electron temperature (T-e) and associated velocity distribution functions (VDFs) are examined and understood in terms of particle energization and randomization processes that vary with exhaust locations. Inside the electron diffusion region (EDR), the electron temperature parallel to the magnetic field (T-e vertical bar parallel to) exhibits a local minimum and the perpendicular temperature (T-e perpendicular to) shows a maximum at the current sheet midplane. In the intermediate exhaust downstream from the EDR and far from the magnetic field pileup region, T-e perpendicular to/T-e parallel to is close to unity and T-e is approximately uniform, but the VDFs are structured: close to the midplane, VDFs are quasi-isotropic, whereas farther away from the midplane, VDFs exhibit field-aligned beams directed toward the midplane. In the far exhaust, T-e generally increases toward the midplane and the pileup region, and the corresponding VDFs show counter-streaming beams. A distinct population with low v(parallel to) and high v(perpendicular to) is prominent in the VDFs around the midplane. Test particle results show that the magnetic curvature near the midplane produces pitch angle scattering to generate quasi-isotropic distributions in the intermediate exhaust. In the far exhaust, electrons with initial high v(parallel to) (v(perpendicular to)) are accelerated mainly through curvature (gradient-B) drift opposite to the electric field, without significant pitch angle scattering. The VDF structures predicted by simulations are observed in magnetotail reconnection measurements, indicating that the energization mechanisms captured in the reported simulations are applicable to magnetotail reconnection with negligible guide field.
C1 [Wang, Shan; Chen, Li-Jen; Bessho, Naoki] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Wang, Shan; Chen, Li-Jen; Bessho, Naoki] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Kistler, Lynn M.; Shuster, Jason R.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Guo, Ruilong] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China.
RP Wang, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.; Wang, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM swang90@umd.edu
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NASA [NNX12AD16G, NNX11AB65G, NNX13AK31G]; NSF [AGS-1202537]; Theory and
Modeling Program of the Magnetospheric Multiscale Mission
FX We acknowledge the instrument teams of Cluster PEACE (PI: Andrew
Fazakerley), CIS (PI: Iannis Dandouras), and FGM (PI: Chris Carr) for
providing plasma and magnetic field data. We acknowledge William
Daughton for his assistance in carrying out the PIC simulations. The
Cluster data are available at Cluster Science Archive (CSA) website
(http://www.cosmos.esa.int/web/csa). The simulation data are available
upon request from the authors. Work at UNH is supported by NASA under
NNX12AD16G, NNX11AB65G, and NNX13AK31G, and by NSF under AGS-1202537.
Work at NASA GSFC is supported by the Theory and Modeling Program of the
Magnetospheric Multiscale Mission.
NR 42
TC 4
Z9 4
U1 3
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2016
VL 121
IS 3
BP 2104
EP 2130
DI 10.1002/2015JA021892
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DK2FV
UT WOS:000374730900020
ER
PT J
AU Walsh, BM
Niehof, J
Collier, MR
Welling, DT
Sibeck, DG
Mozer, FS
Fritz, TA
Kuntz, KD
AF Walsh, B. M.
Niehof, J.
Collier, M. R.
Welling, D. T.
Sibeck, D. G.
Mozer, F. S.
Fritz, T. A.
Kuntz, K. D.
TI Density variations in the Earth's magnetospheric cusps
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Cusp
ID HIGH-ALTITUDE CUSP; SOLAR-WIND; POLAR CUSP; MAGNETIC-FIELD;
MAGNETOSHEATH PLASMA; MAGNETOPAUSE RECONNECTION; CHARGE-TRANSFER;
BOUNDARY-LAYER; ENERGETIC IONS; X-RAYS
AB Seven years of measurements from the Polar spacecraft are surveyed to monitor the variations of plasma density within the magnetospheric cusps. The spacecraft's orbital precession from 1998 through 2005 allows for coverage of both the northern and southern cusps from low altitude out to the magnetopause. In the mid- and high- altitude cusps, plasma density scales well with the solar wind density (n(cusp)/n(sw)approximate to 0.8). This trend is fairly steady for radial distances greater then 4R(E). At low altitudes (r < 4R(E)) the density increases with decreasing altitude and even exceeds the solar wind density due to contributions from the ionosphere. The density of high charge state oxygen (O>+2) also displays a positive trend with solar wind density within the cusp. A multifluid simulation with the Block-Adaptive-Tree Solar Wind Roe-Type Upwind Scheme MHD model was run to monitor the relative contributions of the ionosphere and solar wind plasma within the cusp. The simulation provides similar results to the statistical measurements from Polar and confirms the presence of ionospheric plasma at low altitudes.
C1 [Walsh, B. M.; Fritz, T. A.] Boston Univ, Mech Engn Dept, Boston, MA 02215 USA.
[Walsh, B. M.; Fritz, T. A.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Niehof, J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Collier, M. R.] NASA, Goddard Space Flight Ctr, Planetary Div, Greenbelt, MD USA.
[Welling, D. T.] Univ Michigan, AOSS, Ann Arbor, MI 48109 USA.
[Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD USA.
[Mozer, F. S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Walsh, BM (reprint author), Boston Univ, Mech Engn Dept, Boston, MA 02215 USA.; Walsh, BM (reprint author), Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
EM bwalsh@bu.edu
RI Collier, Michael/I-4864-2013
OI Collier, Michael/0000-0001-9658-6605
FU NASA [NNX14AK41G]
FX Support was given by the NASA grant NNX14AK41G. The authors acknowledge
the use of the SPEDAS analysis software. Analysis of the MHD results was
performed using the Spacepy software library [Morley et al., 2011]. Data
used in this study are openly accessible from NASA's Coordinate Data
Analysis Web (CDAWEB). The CAMMICE/MICS data can be obtained from
http://spacedata.bu.edu/mics.html.
NR 59
TC 1
Z9 1
U1 5
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2016
VL 121
IS 3
BP 2131
EP 2142
DI 10.1002/2015JA022095
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DK2FV
UT WOS:000374730900021
ER
PT J
AU Dunn, WR
Branduardi-Raymont, G
Elsner, RF
Vogt, MF
Lamy, L
Ford, PG
Coates, AJ
Gladstone, GR
Jackman, CM
Nichols, JD
Rae, IJ
Varsani, A
Kimura, T
Hansen, KC
Jasinski, JM
AF Dunn, William R.
Branduardi-Raymont, Graziella
Elsner, Ronald F.
Vogt, Marissa F.
Lamy, Laurent
Ford, Peter G.
Coates, Andrew J.
Gladstone, G. Randall
Jackman, Caitriona M.
Nichols, Jonathan D.
Rae, I. Jonathan
Varsani, Ali
Kimura, Tomoki
Hansen, Kenneth C.
Jasinski, Jamie M.
TI The impact of an ICME on the Jovian X-ray aurora
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Jupiter; X-ray; Aurora; CME; Periodicity; Jovian
ID JUPITERS MIDDLE MAGNETOSPHERE; KELVIN-HELMHOLTZ VORTICES; SOLAR-WIND
CONTROL; RADIO EMISSIONS; ENERGETIC PARTICLE; XMM-NEWTON; BOW SHOCK;
INDUCED COMPRESSIONS; PRECIPITATION; MAGNETOPAUSE
AB We report the first Jupiter X-ray observations planned to coincide with an interplanetary coronal mass ejection (ICME). At the predicted ICME arrival time, we observed a factor of approximate to 8 enhancement in Jupiter's X-ray aurora. Within 1.5h of this enhancement, intense bursts of non-Io decametric radio emission occurred. Spatial, spectral, and temporal characteristics also varied between ICME arrival and another X-ray observation two days later. Gladstone et al. (2002) discovered the polar X-ray hot spot and found it pulsed with 45min quasiperiodicity. During the ICME arrival, the hot spot expanded and exhibited two periods: 26min periodicity from sulfur ions and 12min periodicity from a mixture of carbon/sulfur and oxygen ions. After the ICME, the dominant period became 42min. By comparing Vogt et al. (2011) Jovian mapping models with spectral analysis, we found that during ICME arrival at least two distinct ion populations, from Jupiter's dayside, produced the X-ray aurora. Auroras mapping to magnetospheric field lines between 50 and 70R(J) were dominated by emission from precipitating sulfur ions (S-7+,S-...,S-14+). Emissions mapping to closed field lines between 70 and 120R(J) and to open field lines were generated by a mixture of precipitating oxygen (O-7+,O-8+) and sulfur/carbon ions, possibly implying some solar wind precipitation. We suggest that the best explanation for the X-ray hot spot is pulsed dayside reconnection perturbing magnetospheric downward currents, as proposed by Bunce et al. (2004). The auroral enhancement has different spectral, spatial, and temporal characteristics to the hot spot. By analyzing these characteristics and coincident radio emissions, we propose that the enhancement is driven directly by the ICME through Jovian magnetosphere compression and/or a large-scale dayside reconnection event.
C1 [Dunn, William R.; Branduardi-Raymont, Graziella; Coates, Andrew J.; Rae, I. Jonathan; Varsani, Ali; Jasinski, Jamie M.] Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate Phys, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
[Dunn, William R.; Coates, Andrew J.; Jasinski, Jamie M.] UCL Birkbeck, Ctr Planetary Sci, London, England.
[Elsner, Ronald F.] NASA, Marshall Space Flight Ctr, ZP12, Huntsville, AL USA.
[Vogt, Marissa F.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Lamy, Laurent] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris, Meudon, France.
[Ford, Peter G.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Gladstone, G. Randall] Southwest Res Inst, Space Sci & Engn Div, San Antonio, TX USA.
[Jackman, Caitriona M.] Univ Southampton, Dept Phys & Astron, Southampton, Hants, England.
[Nichols, Jonathan D.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Varsani, Ali] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
[Kimura, Tomoki] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.
[Kimura, Tomoki] RIKEN, Nishina Ctr Accelerator Based Sci, Wako, Saitama, Japan.
[Hansen, Kenneth C.; Jasinski, Jamie M.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Dunn, WR (reprint author), Univ Coll London, Mullard Space Sci Lab, Dept Space & Climate Phys, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.; Dunn, WR (reprint author), UCL Birkbeck, Ctr Planetary Sci, London, England.
EM w.dunn@ucl.ac.uk
RI Vogt, Marissa/C-6237-2014; Nichols, Jonathan/F-5764-2010;
OI Vogt, Marissa/0000-0003-4885-8615; Nichols,
Jonathan/0000-0002-8004-6409; Jackman, Caitriona/0000-0003-0635-7361
FU Science and Technology Facilities Council (STFC); NASA; SAO of NASA
[SV3-73016, NAS8-03060]; UCL-MSSL consolidated grant, from STFC (UK);
CNES; Science and Technology Facilities Council Ernest Rutherford
Fellowship; STFC [ST/ I004084/1]; UK Science and Technology Facilities
Council (STFC) [ST/L000563/1]; Natural and Environmental Research
Council (NERC) [NE/L007495/1]; Japan Society for the Promotion of
Science (JSPS); Chandra Project
FX W.R.D. is supported by a Science and Technology Facilities Council
(STFC) studentship. R.F.E. acknowledges support by NASA's Chandra
Program. P.G.F. was supported by SAO subcontract SV3-73016 of NASA
contract NAS8-03060. A.J.C. acknowledges support via the UCL-MSSL
consolidated grant, from STFC (UK). L.L. is supported by CNES. C.M.J. is
supported by a Science and Technology Facilities Council Ernest
Rutherford Fellowship. J.D.N. was supported by a STFC Advanced
Fellowship (ST/ I004084/1). I.J.R. is funded in part by the UK Science
and Technology Facilities Council (STFC) grant ST/L000563/1 and Natural
and Environmental Research Council (NERC) grant NE/L007495/1. T.K. was
supported by a Grant-in-Aid for Scientific Research from the Japan
Society for the Promotion of Science (JSPS). We warmly thank R. Kraft,
A. Masters, and L. Ray for very helpful discussions. We also thank the
anonymous referee who expressed interest in searching for periodicity at
hard X-rays, which led us to finding possible evidence for it. This work
is mainly based on observations of the NASA Chandra X-ray Observatory
(Observations 12315 and 12316). These observations are available from
the Chandra Data Archive (http://cda.harvard.edu/chaser/). We thank the
Chandra Project for their support. We also used data acquired by the
SECCHI and WAVES experiments of the NASA STEREO spacecraft (available
from http://stereo-ssc.nascom.nasa.gov/data.shtml) and by NASA's Solar
X-ray Imager on the GOES spacecraft (available from
http://sxi.ngdc.noaa.gov/sxi/servlet/sxisearch). We would like to thank
these teams for their support. We would also like to thank both our
reviewers for all their valuable insight and input.
NR 102
TC 2
Z9 2
U1 3
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2016
VL 121
IS 3
BP 2274
EP 2307
DI 10.1002/2015JA021888
PG 34
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DK2FV
UT WOS:000374730900030
PM 27867794
ER
PT J
AU Kimura, T
Kraft, RP
Elsner, RF
Branduardi-Raymont, G
Gladstone, GR
Tao, C
Yoshioka, K
Murakami, G
Yamazaki, A
Tsuchiya, F
Vogt, MF
Masters, A
Hasegawa, H
Badman, SV
Roediger, E
Ezoe, Y
Dunn, WR
Yoshikawa, I
Fujimoto, M
Murray, SS
AF Kimura, T.
Kraft, R. P.
Elsner, R. F.
Branduardi-Raymont, G.
Gladstone, G. R.
Tao, C.
Yoshioka, K.
Murakami, G.
Yamazaki, A.
Tsuchiya, F.
Vogt, M. F.
Masters, A.
Hasegawa, H.
Badman, S. V.
Roediger, E.
Ezoe, Y.
Dunn, W. R.
Yoshikawa, I.
Fujimoto, M.
Murray, S. S.
TI Jupiter's X-ray and EUV auroras monitored by Chandra, XMM-Newton, and
Hisaki satellite
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Jupiter; X-ray; magnetosphere
ID KELVIN-HELMHOLTZ VORTICES; PHOTON IMAGING CAMERA; SOLAR-WIND;
RELATIVISTIC ELECTRONS; SATURNS MAGNETOPAUSE; EMISSION-SPECTRA;
MAGNETIC-FIELD; ULYSSES RADIO; MAGNETOSPHERE; BURSTS
AB Jupiter's X-ray auroral emission in the polar cap region results from particles which have undergone strong field-aligned acceleration into the ionosphere. The origin of precipitating ions and electrons and the time variability in the X-ray emission are essential to uncover the driving mechanism for the high-energy acceleration. The magnetospheric location of the source field line where the X-ray is generated is likely affected by the solar wind variability. However, these essential characteristics are still unknown because the long-term monitoring of the X-rays and contemporaneous solar wind variability has not been carried out. In April 2014, the first long-term multiwavelength monitoring of Jupiter's X-ray and EUV auroral emissions was made by the Chandra X-ray Observatory, XMM-Newton, and Hisaki satellite. We find that the X-ray count rates are positively correlated with the solar wind velocity and insignificantly with the dynamic pressure. Based on the magnetic field mapping model, a half of the X-ray auroral region was found to be open to the interplanetary space. The other half of the X-ray auroral source region is magnetically connected with the prenoon to postdusk sector in the outermost region of the magnetosphere, where the Kelvin-Helmholtz (KH) instability, magnetopause reconnection, and quasiperiodic particle injection potentially take place. We speculate that the high-energy auroral acceleration is associated with the KH instability and/or magnetopause reconnection. This association is expected to also occur in many other space plasma environments such as Saturn and other magnetized rotators.
C1 [Kimura, T.; Yoshioka, K.; Murakami, G.; Yamazaki, A.; Hasegawa, H.; Fujimoto, M.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.
[Kimura, T.] RIKEN, Nishina Ctr Accelerator Based Sci, Saitama, Japan.
[Kimura, T.; Kraft, R. P.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Elsner, R. F.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Branduardi-Raymont, G.; Dunn, W. R.] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
[Gladstone, G. R.] SW Res Inst, Dept Space Studies, Boulder, CO USA.
[Tao, C.] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, Toulouse, France.
[Tsuchiya, F.] Tohoku Univ, Planetary Plasma & Atmospher Res Ctr, Sendai, Miyagi 980, Japan.
[Vogt, M. F.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Masters, A.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, Fac Nat Sci, London, England.
[Badman, S. V.] Univ Lancaster, Dept Phys, Lancaster, England.
[Roediger, E.] Univ Hamburg, Hamburger Sternwarte, Hamburg, Germany.
[Ezoe, Y.] Tokyo Metropolitan Univ, Tokyo 158, Japan.
[Yoshikawa, I.] Univ Tokyo, Dept Complex Sci & Engn, Chiba, Japan.
[Fujimoto, M.] Tokyo Inst Technol, Earth Life Sci Inst, Tokyo 152, Japan.
RP Kimura, T (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan.; Kimura, T (reprint author), RIKEN, Nishina Ctr Accelerator Based Sci, Saitama, Japan.; Kimura, T (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM tomoki.kimura@riken.jp
RI Hasegawa, Hiroshi/A-1192-2007; Vogt, Marissa/C-6237-2014
OI Hasegawa, Hiroshi/0000-0002-1172-021X; Vogt, Marissa/0000-0003-4885-8615
FU Japan Society for the Promotion of Science (JSPS)
FX T.K. was supported by a grant-in-aid for Scientific Research from the
Japan Society for the Promotion of Science (JSPS). The data of Hisaki
satellite are archived in the Data Archives and Transmission System
(DARTS) JAXA. Individuals may request the data by writing to Timoki
Kimura (tomoki.kimura@riken.jp).
NR 65
TC 2
Z9 2
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2016
VL 121
IS 3
BP 2308
EP 2320
DI 10.1002/2015JA021893
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DK2FV
UT WOS:000374730900031
ER
PT J
AU Ruhunusiri, S
Halekas, JS
Connerney, JEP
Espley, JR
McFadden, JP
Mazelle, C
Brain, D
Collinson, G
Harada, Y
Larson, DE
Mitchell, DL
Livi, R
Jakosky, BM
AF Ruhunusiri, Suranga
Halekas, J. S.
Connerney, J. E. P.
Espley, J. R.
McFadden, J. P.
Mazelle, C.
Brain, D.
Collinson, G.
Harada, Y.
Larson, D. E.
Mitchell, D. L.
Livi, R.
Jakosky, B. M.
TI MAVEN observation of an obliquely propagating low-frequency wave
upstream of Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE MAVEN; Mars; upstream waves; pickup ions; bow-shock reflected ions
ID ION-CYCLOTRON WAVES; COMET GIACOBINI-ZINNER; SOLAR-WIND; BOW SHOCK;
ELECTROMAGNETIC-WAVES; HYDROMAGNETIC-WAVES; ISEE-2 OBSERVATIONS;
REFLECTED IONS; MARTIAN SHOCK; REGION
AB We report Mars Atmosphere and Volatile EvolutioN mission observations of a large amplitude low-frequency plasma wave that propagated oblique to the ambient magnetic field upstream of Mars along with a non-solar-wind plasma component that had a flow velocity perpendicular to the magnetic field. We consider nine possibilities for this wave that include various combinations of its propagation direction, polarization in the solar wind frame, and ion source responsible for its generation. Using the observed wave parameters and the measured plasma parameters as constraints, we uniquely identify the wave by systematically discarding these possibilities. We determine that the wave is a right-hand polarized wave that propagated upstream in the solar wind frame. We find two possibilities for the ion source that can be responsible for this wave generation. They are either newly born pickup protons or reflected solar wind protons from the bow shock. We determine that the observed non-solar-wind component is notresponsible for the wave generation, and it is likely that the non-solar-wind component was merely perturbed by the passage of the wave.
C1 [Ruhunusiri, Suranga; Halekas, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Connerney, J. E. P.; Espley, J. R.; Collinson, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[McFadden, J. P.; Harada, Y.; Larson, D. E.; Mitchell, D. L.; Livi, R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Mazelle, C.] CNRS, IRAP, Toulouse, France.
[Mazelle, C.] Univ Toulouse 3, F-31062 Toulouse, France.
[Brain, D.; Jakosky, B. M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
RP Ruhunusiri, S (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
EM suranga-ruhunusiri@uiowa.edu
OI Halekas, Jasper/0000-0001-5258-6128
FU NASA; CNES
FX This work was supported by NASA and was partially supported by the CNES.
MAVEN data are publicly available through the Planetary Data System.
NR 49
TC 7
Z9 7
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2016
VL 121
IS 3
BP 2374
EP 2389
DI 10.1002/2015JA022306
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DK2FV
UT WOS:000374730900036
ER
PT J
AU Burke, WJ
Martinis, CR
Lai, PC
Gentile, LC
Sullivan, C
Pfaff, RF
AF Burke, W. J.
Martinis, C. R.
Lai, P. C.
Gentile, L. C.
Sullivan, C.
Pfaff, R. F.
TI C/NOFS observations of electromagnetic coupling between magnetically
conjugate MSTID structures
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE medium-scale traveling ionospheric disturbances; Alfven wave detection
at midlatitudes; interhemispheric coupling
ID TRAVELING IONOSPHERIC DISTURBANCES; NIGHTTIME MIDLATITUDE IONOSPHERE;
SPORADIC-E-LAYERS; MU RADAR; F-LAYER; ARECIBO; INSTABILITY; SATELLITE;
IMAGES
AB This report demonstrates empirically that couplings between magnetically conjugate medium-scale traveling ionospheric disturbances (MSTIDs) are electromagnetic in nature. This is accomplished by comparing plasma density, electric, and magnetic perturbations sampled simultaneously by sensors on the Communication/Navigation Outage Forecasting System (C/NOFS) satellite. During the period of interest on 17 February 2010, C/NOFS made three consecutive orbits while magnetically conjugate to the field of view of an all-sky imager located at El Leoncito, Argentina (31.8 degrees S, 69.3 degrees W). Imaged 630.0nm airglow was characterized by alternating bands of relatively bright and dark emissions that were aligned from northeast to southwest and propagated toward the northwest, characteristic of MSTIDs in the southern hemisphere. Measurable Poynting fluxes flow along the Earth's magnetic field (S-||) from generator to load hemispheres. While S-|| was predominantly away from the ionosphere above El Leoncito, interhemispheric energy flows were not one-way streets. Measured Poynting flux intensities diminished with time over the three C/NOFS passes, suggesting that source mechanisms of MSTIDs were absent or that initial impedance mismatches between the two hemispheres approached an equilibrium status.
C1 [Burke, W. J.; Lai, P. C.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02167 USA.
[Martinis, C. R.; Sullivan, C.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Gentile, L. C.] Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, NM USA.
[Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Gentile, LC (reprint author), Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, NM USA.
EM louise.gentile@kirtland.af.mil
FU Boston College [FA9453-12-C-0205, FA8712-10-C-0001]; NSF Aeronomy
[1123222]; Air Force Office of Scientific Research
FX The authors express their gratitude to Carmen Liebrecht of the NASA
Goddard Space Flight Center for going the extra mile to make the VEFI
electric and magnetic field data available to us. We also thank Patrick
Roddy of the Air Force Research Laboratory who provided the C/NOFS PLP
plasma densities used in this report. C/NOFS PLP data are available from
Roddy upon request. VEFI data from the first 3 years of the C/NOFS
mission are available on the CDA website with plans to make later VEFI
data available. Observations from the Boston University All-sky Imagers
are available at http://sirius.bu.edu/. CINDI data are available at
http://cindispace.utdallas.edu. W.J.B. received support under contracts
FA9453-12-C-0205 and FA8712-10-C-0001 with Boston College. C.R.M.
acknowledges the support of NSF Aeronomy grant 1123222 and Air Force
Office of Scientific Research grant for DURIP instrumentation.
NR 40
TC 3
Z9 3
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAR
PY 2016
VL 121
IS 3
BP 2569
EP 2582
DI 10.1002/2015JA021965
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DK2FV
UT WOS:000374730900050
ER
PT J
AU Benedict, M
Lakshminarayan, V
Pino, J
Chopra, I
AF Benedict, Moble
Lakshminarayan, Vinod
Pino, Johnathan
Chopra, Inderjit
TI Aerodynamics of a Small-Scale Vertical-Axis Wind Turbine with Dynamic
Blade Pitching
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 54th AIAA/ASME/ASCE/AHS/ASC Structures, Structural Dynamics, and
Materials Conference
CY APR 08-11, 2013
CL Boston, MA
SP AIAA, ASME, ASCE, AHS, ASC
ID COMPUTATIONAL PHYSICS
AB This paper describes the systematic experimental and computational studies performed to investigate the performance of a small-scale vertical-axis wind turbine using dynamic blade pitching. A vertical-axis wind turbine prototype with a simplified blade pitch mechanism was designed, built, and tested in the wind tunnel to understand the role of pitch kinematics in turbine aerodynamic efficiency. Acomputational fluid dynamics model was developed, and the model predictions correlated well with test data. Both experimental and computational fluid dynamics studies showed that the turbine efficiency is a strong function of blade pitching amplitude, with the highest efficiency occurring around +/- 20 to +/- 25 deg amplitude. The optimum tip-speed ratio depends on the blade pitch kinematics, and it decreases with increasing pitch amplitude for the symmetric blade pitching case. A computational fluid dynamics analysis showed that the blade extracted all the power in the frontal half of the circular trajectory; however, it lost power into the flow in the rear half: one key reason for this being the large virtual camber and incidence induced by the flow curvature effects, which slightly enhanced the power extraction in the frontal half but increased the power loss in the rear half. The maximum achievable C-P of the turbine increased with higher Reynolds numbers; however, the fundamental flow physics remained relatively the same, irrespective of the operating Reynolds number. This study clearly indicates the potential for major improvements in vertical-axis wind turbine performance with novel blade kinematics, a lower chord/radius ratio, and using cambered blades.
C1 [Benedict, Moble] Texas A&M Univ, Dept Aerosp Engn, College Stn, TX 77843 USA.
[Lakshminarayan, Vinod] NASA, Ames Res Ctr, Sci & Technol Corp, Moffett Field, CA 94035 USA.
[Pino, Johnathan] Univ Maryland, Dept Aerosp Engn, College Pk, MD 20742 USA.
[Chopra, Inderjit] Univ Maryland, Dept Aerosp Engn, Alfred Gessow Rotorcraft Ctr, College Pk, MD 20742 USA.
RP Benedict, M (reprint author), Texas A&M Univ, Dept Aerosp Engn, College Stn, TX 77843 USA.
NR 16
TC 0
Z9 0
U1 2
U2 6
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD MAR
PY 2016
VL 54
IS 3
BP 924
EP 935
DI 10.2514/1.J052979
PG 12
WC Engineering, Aerospace
SC Engineering
GA DL1XF
UT WOS:000375425800010
ER
PT J
AU Pak, CG
AF Pak, Chan-gi
TI Wing Shape Sensing from Measured Strain
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 53rd AIAA Aerospace Sciences Meeting / AIAA Atmospheric Flight Mechanics
Conference / 17th AIAA Non-Deterministic Approaches Conference / AIAA
Science and Technology Forum / AIAA Infotech at Aerospace Conference
CY JAN 05-09, 2015
CL Kissimmee, FL
SP AIAA
AB A new two-step theory is investigated for predicting the deflection and slope of an entire structure using measured strain at discrete locations. In the first step, a measured strain is fitted using a piecewise least-squares curve fitting method together with the cubic spline technique. These fitted strains are integrated twice to obtain deflection data along the optical fibers. In the second step, computed deflection along the optical fibers is combined with a finite-element model of the structure in order to interpolate and extrapolate the deflection and slope of the entire structure through the use of the System Equivalent Reduction and Expansion Process. The theory is first validated on a computational model, a cantilevered rectangular plate wing. The theory is then applied to test data from a cantilevered swept-plate wing model. Computed results are compared with finite-element results, results using another strain-based method, and photogrammetry data. In general, excellent matching between the target and computed values are accomplished in this study.
C1 [Pak, Chan-gi] NASA, Armstrong Flight Res Ctr, Aerostruct Branch, POB 273,Mailstop 48202A, Edwards AFB, CA 93523 USA.
RP Pak, CG (reprint author), NASA, Armstrong Flight Res Ctr, Aerostruct Branch, POB 273,Mailstop 48202A, Edwards AFB, CA 93523 USA.
NR 20
TC 0
Z9 0
U1 3
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD MAR
PY 2016
VL 54
IS 3
BP 1064
EP 1073
DI 10.2514/1.J053986
PG 10
WC Engineering, Aerospace
SC Engineering
GA DL1XF
UT WOS:000375425800021
ER
PT J
AU Scholten, WD
Hartl, DJ
Turner, TL
Kidd, RT
AF Scholten, William D.
Hartl, Darren J.
Turner, Travis L.
Kidd, Reggie T.
TI Development and Analysis-Driven Optimization of Superelastic Slat-Cove
Fillers for Airframe Noise Reduction
SO AIAA JOURNAL
LA English
DT Article
ID SHAPE-MEMORY ALLOYS; NUMERICAL SIMULATIONS; TRAILING-EDGE; BEHAVIOR;
FLOW
AB Airframe noise constitutes a significant component of the total noise generated by transport aircraft during low-speed maneuvers, such as approach and landing; the leading-edge slat is a major source. Previous work has shown that the noise produced by the slat can be mitigated through the use of a slat-cove filler. Results from the initial prototype testing led to slat-cove filler concepts that incorporated a segmented structure and superelastic shape-memory alloy materials. A finite-element analysis model, based on the physical prototypes (with a shape profile optimized for maximum noise reduction), was created and used to analyze the slat-cove filler response to aerodynamic and slat retraction loads with the goal of optimization. The objective was minimization of the actuation force needed to retract the slat/slat-cove filler assembly subject to constraints that involved aeroelastic deflection of the slat-cove filler when deployed, maximum stress in the shape-memory alloy flexures, and the required ability of the slat-cove filler to deploy autonomously during slat deployment. The design variables considered included shape-memory alloy flexure thicknesses and lengths of various slat-cove filler components. Design of experiment studies were conducted and used to guide the subsequent optimization. From the optimization, it was found that a monolithic shape-memory alloy slat-cove filler minimized the actuation force while satisfying design constraints, which was consistent with prototype testing results.
C1 [Scholten, William D.; Hartl, Darren J.] Texas A&M Univ, Dept Aerosp Engn, Texas Inst Intelligent Mat & Struct, College Stn, TX 77843 USA.
[Turner, Travis L.] NASA, Langley Res Ctr, Struct Acoust Branch, Hampton, VA 23681 USA.
[Kidd, Reggie T.] Analyt Mech Associates, Aeronaut Syst Engn Branch, Hampton, VA 23681 USA.
RP Scholten, WD (reprint author), Texas A&M Univ, Dept Aerosp Engn, Texas Inst Intelligent Mat & Struct, College Stn, TX 77843 USA.
NR 33
TC 1
Z9 1
U1 11
U2 12
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD MAR
PY 2016
VL 54
IS 3
BP 1074
EP 1090
DI 10.2514/1.J054011
PG 17
WC Engineering, Aerospace
SC Engineering
GA DL1XF
UT WOS:000375425800022
ER
PT J
AU Koklu, M
AF Koklu, Mehti
TI Effect of a Coanda Extension on the Performance of a Sweeping-Jet
Actuator
SO AIAA JOURNAL
LA English
DT Article
C1 [Koklu, Mehti] NASA, Langley Res Ctr, Flow Phys & Control Branch, MS 170, Hampton, VA 23681 USA.
RP Koklu, M (reprint author), NASA, Langley Res Ctr, Flow Phys & Control Branch, MS 170, Hampton, VA 23681 USA.
FU NASA Fixed Wing Project
FX The author would like to thank the NASA Fixed Wing Project for funding
the research, and the following individuals for their support: Catherine
McGinley, Luther Jenkins, John Lin, and Latunia Melton.
NR 16
TC 0
Z9 0
U1 2
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD MAR
PY 2016
VL 54
IS 3
BP 1125
EP 1128
DI 10.2514/1.J054448
PG 4
WC Engineering, Aerospace
SC Engineering
GA DL1XF
UT WOS:000375425800027
ER
PT J
AU Romero-Mangado, J
Nordlund, D
Soberon, F
Deane, G
Maughan, K
Sainio, S
Singh, G
Daniels, S
Saunders, IT
Loftus, D
Meyyappan, M
Koehne, J
Gandhiraman, RP
AF Romero-Mangado, Jaione
Nordlund, Dennis
Soberon, Felipe
Deane, Graham
Maughan, Kevin
Sainio, Sami
Singh, Gurusharan
Daniels, Stephen
Saunders, Ian T.
Loftus, David
Meyyappan, M.
Koehne, Jessica
Gandhiraman, Ram P.
TI Morphological and chemical changes of aerosolized E-coli treated with a
dielectric barrier discharge
SO BIOINTERPHASES
LA English
DT Article
ID TRANSFORM INFRARED-SPECTROSCOPY; GRAM-NEGATIVE BACTERIA; K-EDGE XANES;
PHOTOCATALYTIC INACTIVATION; OUTER-MEMBRANE; FTIR-SPECTROSCOPY; AIRBORNE
BACTERIA; ORGANIC NITROGEN; AIR; PLASMA
AB This study presents the morphological and chemical modification of the cell structure of aerosolized Escherichia coli treated with a dielectric barrier discharge (DBD). Exposure to DBD results in severe oxidation of the bacteria, leading to the formation of hydroxyl groups and carbonyl groups and a significant reduction in amine functionalities and phosphate groups. Near edge x-ray absorption fine structure (NEXAFS) measurements confirm the presence of additional oxide bonds upon DBD treatment, suggesting oxidation of the outer layer of the cell wall. Electron microscopy images show that the bacteria undergo physical distortion to varying degrees, resulting in deformation of the bacterial structure. The electromagnetic field around the DBD coli causes severe damage to the cell structure, possibly resulting in leakage of vital cellular materials. The oxidation and chemical modification of the bacterial components are evident from the Fourier transform infrared spectroscopy and NEXAFS results. The bacterial reculture experiments confirm inactivation of airborne E. coli upon treating with DBD. (C) 2016 Author(s).
C1 [Romero-Mangado, Jaione; Saunders, Ian T.; Loftus, David; Meyyappan, M.; Koehne, Jessica; Gandhiraman, Ram P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Nordlund, Dennis] SLAC Natl Accelerator Lab, Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA 94025 USA.
[Soberon, Felipe; Deane, Graham; Maughan, Kevin] Novaerus Inc, 111 N Canal St Suite 165, Chicago, IL 60606 USA.
[Sainio, Sami] Aalto Univ, Sch Elect Engn, Dept Elect Engn & Automat, Espoo 02150, Finland.
[Singh, Gurusharan; Daniels, Stephen] Dublin City Univ, Natl Ctr Plasma Sci & Technol, Dublin 9, Ireland.
[Gandhiraman, Ram P.] Univ Space Res Assoc, Mountain View, CA 94043 USA.
RP Gandhiraman, RP (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.; Gandhiraman, RP (reprint author), Univ Space Res Assoc, Mountain View, CA 94043 USA.
EM ramprasad.gandhiraman@nasa.gov
RI Nordlund, Dennis/A-8902-2008;
OI Nordlund, Dennis/0000-0001-9524-6908; Daniels,
Stephen/0000-0002-5987-9924
FU U.S. Department of Energy, Office of Science, Office of Basic Energy
Sciences [DE-AC02-76SF00515]
FX J. Romero-Mangado is a Science and Technology Corporation employee
subcontracted to work at NASA Ames Research Center. Ian T. Saunders was
a student intern from Norfolk State University. Use of the Stanford
Synchrotron Radiation Lightsource, SLAC National Accelerator Laboratory,
is supported by the U.S. Department of Energy, Office of Science, Office
of Basic Energy Sciences under Contract No. DE-AC02-76SF00515. The
authors thank the support from the beamline staff at SSRL, Jun-Sik Lee,
and Glen Kerr. The contents of this publication are solely the
responsibility of the authors and do not necessarily represent the
official views of NIGMS or NIH.
NR 61
TC 0
Z9 0
U1 1
U2 8
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1934-8630
EI 1559-4106
J9 BIOINTERPHASES
JI Biointerphases
PD MAR
PY 2016
VL 11
IS 1
AR 011009
DI 10.1116/1.4941367
PG 8
WC Biophysics; Materials Science, Biomaterials
SC Biophysics; Materials Science
GA DK5TB
UT WOS:000374982200009
PM 26872580
ER
PT J
AU Waple, AM
Champion, SM
Kunkel, KE
Tilmes, C
AF Waple, Anne M.
Champion, Sarah M.
Kunkel, Kenneth E.
Tilmes, Curt
TI Innovations in information management and access for assessments
SO CLIMATIC CHANGE
LA English
DT Article
ID GLOBAL CHANGE INFORMATION; PROVENANCE
AB The third National Climate Assessment (NCA3) included goals for becoming a more timely, inclusive, rigorous, and sustained process, and for serving a wider variety of decision makers. In order to accomplish these goals, it was necessary to deliberately design an information management strategy that could serve multiple stakeholders and manage different types of information - from highly mature government-supported climate science data, to isolated practitioner-generated case study information - and to do so in ways that are consistent and appropriate for a highly influential assessment. Meeting the information management challenge for NCA3 meant balancing relevance and authority, complexity and accessibility, inclusivity and rigor. Increasing traceability of data behind figures and graphics, designing a public-facing website, managing hundreds of technical inputs to the NCA, and producing guidance for over 300 participants on meeting the Information Quality Act were all aspects of a deliberate, multi-faceted, and strategic information management approach that nonetheless attempted to be practical and usable for a variety of participants and stakeholders.
C1 [Waple, Anne M.] Second Nat, Boston, MA USA.
[Champion, Sarah M.; Kunkel, Kenneth E.] N Carolina State Univ, NOAA, Cooperat Inst Climate & Satellites NC, Natl Ctr Environm Informat, Asheville, NC USA.
[Tilmes, Curt] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Waple, AM (reprint author), Second Nat, Boston, MA USA.
EM awaple@secondnature.org
RI Kunkel, Kenneth/C-7280-2015
OI Kunkel, Kenneth/0000-0001-6667-7047
FU NOAA through Cooperative Institute for Climate and Satellites North
Carolina [NA14NES432003]
FX This work was partially supported by NOAA through the Cooperative
Institute for Climate and Satellites North Carolina under Cooperative
Agreement NA14NES432003.
NR 14
TC 2
Z9 2
U1 5
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0165-0009
EI 1573-1480
J9 CLIMATIC CHANGE
JI Clim. Change
PD MAR
PY 2016
VL 135
IS 1
BP 69
EP 83
DI 10.1007/s10584-015-1588-7
PG 15
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DL2LG
UT WOS:000375465700006
ER
PT J
AU Chern, JD
Tao, WK
Lang, SE
Matsui, T
Li, JLF
Mohr, KI
Skofronick-Jackson, GM
Peters-Lidard, CD
AF Chern, Jiun-Dar
Tao, Wei-Kuo
Lang, Stephen E.
Matsui, Toshihisa
Li, J. -L. F.
Mohr, Karen I.
Skofronick-Jackson, Gail M.
Peters-Lidard, Christa D.
TI Performance of the Goddard multiscale modeling framework with Goddard
ice microphysical schemes
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
DE superparameterization; MMF; microphysics; CloudSat
ID CLOUD-RESOLVING MODEL; MADDEN-JULIAN OSCILLATION; SIMULATED RADAR
REFLECTIVITIES; CLIMATE MODEL; CONVECTIVE SYSTEMS; PART I;
SUPERPARAMETERIZED CAM; BULK PARAMETERIZATION; MIDLATITUDE CYCLONES;
MICROSCALE STRUCTURE
AB The multiscale modeling framework (MMF), which replaces traditional cloud parameterizations with cloud-resolving models (CRMs) within a host atmospheric general circulation model (GCM), has become a new approach for climate modeling. The embedded CRMs make it possible to apply CRM-based cloud microphysics directly within a GCM. However, most such schemes have never been tested in a global environment for long-term climate simulation. The benefits of using an MMF to evaluate rigorously and improve microphysics schemes are here demonstrated. Four one-moment microphysical schemes are implemented into the Goddard MMF and their results validated against three CloudSat/CALIPSO cloud ice products and other satellite data. The new four-class (cloud ice, snow, graupel, and frozen drops/hail) ice scheme produces a better overall spatial distribution of cloud ice amount, total cloud fractions, net radiation, and total cloud radiative forcing than earlier three-class ice schemes, with biases within the observational uncertainties. Sensitivity experiments are conducted to examine the impact of recently upgraded microphysical processes on global hydrometeor distributions. Five processes dominate the global distributions of cloud ice and snow amount in long-term simulations: (1) allowing for ice supersaturation in the saturation adjustment, (2) three additional correction terms in the depositional growth of cloud ice to snow, (3) accounting for cloud ice fall speeds, (4) limiting cloud ice particle size, and (5) new size-mapping schemes for snow and graupel. Despite the cloud microphysics improvements, systematic errors associated with subgrid processes, cyclic lateral boundaries in the embedded CRMs, and momentum transport remain and will require future improvement.
C1 [Chern, Jiun-Dar; Tao, Wei-Kuo; Lang, Stephen E.; Matsui, Toshihisa; Skofronick-Jackson, Gail M.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD USA.
[Chern, Jiun-Dar; Matsui, Toshihisa] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Lang, Stephen E.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Li, J. -L. F.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Mohr, Karen I.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Atmospheres, Greenbelt, MD USA.
[Peters-Lidard, Christa D.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Hydrospher & Biospher Sci, Greenbelt, MD USA.
RP Chern, JD (reprint author), NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD USA.; Chern, JD (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM Jiun-dar.chern-1@nasa.gov
RI Peters-Lidard, Christa/E-1429-2012
OI Peters-Lidard, Christa/0000-0003-1255-2876
FU NASA
FX This research was supported by the NASA Modeling, Analysis, and
Prediction (MAP) Program and the NASA Precipitation Measurement Missions
(PMM). The authors are grateful to David B. Considine and Ramesh Kakar
at NASA HQ for their support of this research. Acknowledgment is also
made to the NASA Goddard Space Flight Center and NASA Ames Research
Center computing facilities and to Tsengdar Lee at NASA HQ for the
computational resources used in this research. CloudSat data were
acquired through the CloudSat Data processing Center at Colorado State
University (http://cloudsat.cira.colostate.edu). CloudSat/CALIPSO cloud
fractions were obtained from https://climatedataguide.ucar.edu and.
CERES-EBAF data were acquired from the NASA Langley Research Center
(http://ceres-tool.larc.nasa.gov). GPCP Precipitation data were provided
by the NOAA/OAR/ESRL from their web site at
http://www.esrl.noaa.gov/psd/.
NR 137
TC 2
Z9 2
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PD MAR
PY 2016
VL 8
IS 1
BP 66
EP 95
DI 10.1002/2015MS000469
PG 30
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DK2UP
UT WOS:000374770200004
ER
PT J
AU Daleu, CL
Plant, RS
Woolnough, SJ
Sessions, S
Herman, MJ
Sobel, A
Wang, S
Kim, D
Cheng, A
Bellon, G
Peyrille, P
Ferry, F
Siebesma, P
van Ulft, L
AF Daleu, C. L.
Plant, R. S.
Woolnough, S. J.
Sessions, S.
Herman, M. J.
Sobel, A.
Wang, S.
Kim, D.
Cheng, A.
Bellon, G.
Peyrille, P.
Ferry, F.
Siebesma, P.
van Ulft, L.
TI Intercomparison of methods of coupling between convection and
large-scale circulation: 2. Comparison over nonuniform surface
conditions
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
DE tropical convection; large-scale parameterized dynamics
ID CLOUD-RESOLVING MODEL; TEMPERATURE-GRADIENT APPROXIMATION; TROPICAL DEEP
CONVECTION; WATER-VAPOR; MOIST CONVECTION; SINGLE-COLUMN; SYSTEM;
PRECIPITATION; SIMULATIONS; SENSITIVITY
AB As part of an international intercomparison project, the weak temperature gradient (WTG) and damped gravity wave (DGW) methods are used to parameterize large-scale dynamics in a set of cloud-resolving models (CRMs) and single column models (SCMs). The WTG or DGW method is implemented using a configuration that couples a model to a reference state defined with profiles obtained from the same model in radiative-convective equilibrium. We investigated the sensitivity of each model to changes in SST, given a fixed reference state. We performed a systematic comparison of the WTG and DGW methods in different models, and a systematic comparison of the behavior of those models using the WTG method and the DGW method. The sensitivity to the SST depends on both the large-scale parameterization method and the choice of the cloud model. In general, SCMs display a wider range of behaviors than CRMs. All CRMs using either the WTG or DGW method show an increase of precipitation with SST, while SCMs show sensitivities which are not always monotonic. CRMs using either the WTG or DGW method show a similar relationship between mean precipitation rate and column-relative humidity, while SCMs exhibit a much wider range of behaviors. DGW simulations produce large-scale velocity profiles which are smoother and less top-heavy compared to those produced by the WTG simulations. These large-scale parameterization methods provide a useful tool to identify the impact of parameterization differences on model behavior in the presence of two-way feedback between convection and the large-scale circulation.
C1 [Daleu, C. L.; Plant, R. S.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Woolnough, S. J.] Univ Reading, Dept Meteorol, Natl Ctr Atmospher Sci, Reading, Berks, England.
[Sessions, S.; Herman, M. J.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM USA.
[Sobel, A.] Columbia Univ, Dept Environm Sci, New York, NY USA.
[Wang, S.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Kim, D.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Cheng, A.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23665 USA.
[Bellon, G.] Univ Auckland, Dept Phys, Auckland, New Zealand.
[Peyrille, P.; Ferry, F.] Meteo France, Toulouse, France.
[Siebesma, P.; van Ulft, L.] Royal Netherlands Meteorol Inst, POB 201, NL-3730 AE De Bilt, Netherlands.
[Siebesma, P.] Delft Univ Technol, Delft, Netherlands.
RP Daleu, CL (reprint author), Univ Reading, Dept Meteorol, Reading, Berks, England.
EM c.daleu@reading.ac.uk
RI Wang, Shuguang/C-2893-2011; Sobel, Adam/K-4014-2015;
OI Wang, Shuguang/0000-0003-1861-9285; Sobel, Adam/0000-0003-3602-0567;
Plant, Robert/0000-0001-8808-0022; Bellon, Gilles/0000-0003-3981-1225
FU NERC [NE/K004034/1]; NCAS, a NERC collaborative center; U.S. National
Science Foundation [AGS-1056254, AGS-1342001, 1342001]; NM EPSCoR; NSF
[AGS-1062206]; NASA [NNX13AM18G]; Korea Meteorological Administration
Research and Development Program [CATER 2013-3142]; DOE Atmospheric
System Research Program [DE-SC0005450, DE-SC0008779]; European
Commission's Seventh Framework Programme [282672]
FX C. L. D., R. S. P., and S. J. W. thank the UK Met Office for the
availability of the LEM at version 2.4 and SCM version 7.8 of the UK Met
Office Unified Model. C. L. D. was supported by NERC, grant
NE/K004034/1. S. J. W. was supported by the NCAS, a NERC collaborative
center. The New Mexico Tech group thanks Carlos Lopez Carrillo, Ana
Juracic, and Stipo Sentic for model output analysis and for continual
discussions on the tropical atmosphere. We also thank Raul
Morales-Juberias for use of the Pelican beowulf cluster. S. L. S.
acknowledges support from U.S. National Science Foundation grants
AGS-1056254 and AGS-1342001, and NM EPSCoR. M. J. H. was supported by
U.S. National Science Foundation grant 1342001. A. H. S. and S. W. were
partially supported by NSF grant AGS-1062206. The WRF simulations were
carried out on the Yeti Shared HPC Cluster at Columbia University. G. B.
thanks Isabelle Beau, Antoinette Alias, David Saint-Martin, Jean-Yves
Grandpeix, Marie-Pierre Lefebvre, and the CNRS/INSU-LEFE project DEPHY
and the European Union FP7 project EMBRACE. D. K. appreciates the
NASA/GISS modeling group, especially Maxwell Kelley, Mao-Sung Yao, and
Anthony Del Genio, for their invaluable and unlimited supports. D. K.
and A. H. S. were supported by the NASA grant NNX13AM18G and the Korea
Meteorological Administration Research and Development Program under
grant CATER 2013-3142. LaRC CRM-IPHOC was partially supported by DOE
Atmospheric System Research Program under Interagency agreements
DE-SC0005450 and DE-SC0008779. The computation resources were provided
by SSAI Icluster and LaRC Kcluster. P. P., A. P. S., and L. U. were
supported by the European Commission's Seventh Framework Programme,
under grant agreement 282672, EMBRACE project. Data used for this
research are available upon request from the corresponding author;
please send requests via email to c.daleu@reading.ac.uk.
NR 41
TC 0
Z9 0
U1 2
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PD MAR
PY 2016
VL 8
IS 1
BP 387
EP 405
DI 10.1002/2015MS000570
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DK2UP
UT WOS:000374770200019
ER
PT J
AU Yue, Q
Kahn, BH
Fetzer, EJ
Schreier, M
Wong, S
Chen, XH
Huang, XL
AF Yue, Qing
Kahn, Brian H.
Fetzer, Eric J.
Schreier, Mathias
Wong, Sun
Chen, Xiuhong
Huang, Xianglei
TI Observation-Based Longwave Cloud Radiative Kernels Derived from the
A-Train
SO JOURNAL OF CLIMATE
LA English
DT Article
ID GENERAL-CIRCULATION MODELS; CLIMATE FEEDBACKS; BUDGET EXPERIMENT; MODIS;
PRODUCTS; ISCCP; ATMOSPHERES; INSTRUMENT; SATELLITE; MISSION
AB The authors present a new method to derive both the broadband and spectral longwave observation-based cloud radiative kernels (CRKs) using cloud radiative forcing (CRF) and cloud fraction (CF) for different cloud types using multisensor A-Train observations and MERRA data collocated on the pixel scale. Both observation-based CRKs and model-based CRKs derived from the Fu-Liou radiative transfer model are shown. Good agreement between observation-and model-derived CRKs is found for optically thick clouds. For optically thin clouds, the observation-based CRKs show a larger radiative sensitivity at TOA to cloud-cover change than model-derived CRKs. Four types of possible uncertainties in the observed CRKs are investigated: 1) uncertainties in Moderate Resolution Imaging Spectroradiometer cloud properties, 2) the contributions of clear-sky changes to the CRF, 3) the assumptions regarding clear-sky thresholds in the observations, and 4) the assumption of a single-layer cloud. The observation-based CRKs show the TOA radiative sensitivity of cloud types to unit cloud fraction change as observed by the A-Train. Therefore, a combination of observation-based CRKs with cloud changes observed by these instruments over time will provide an estimate of the short-term cloud feedback by maintaining consistency between CRKs and cloud responses to climate variability.
C1 [Yue, Qing; Kahn, Brian H.; Fetzer, Eric J.; Schreier, Mathias; Wong, Sun] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 233-302C, Pasadena, CA 91109 USA.
[Chen, Xiuhong; Huang, Xianglei] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Yue, Q (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 233-302C, Pasadena, CA 91109 USA.
EM qing.yue@jpl.nasa.gov
RI Huang, Xianglei/G-6127-2011; Yue, Qing/F-4619-2017
OI Huang, Xianglei/0000-0002-7129-614X; Yue, Qing/0000-0002-3559-6508
FU National Aeronautics and Space Administration; NASA's Making Earth
Science Data Records for Use in Research Environments (MEaSUREs)
program; AIRS project at JPL; NASA [NNX14AJ50G]
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. QY,
BHK, EJF, MS, and SW were supported by NASA's Making Earth Science Data
Records for Use in Research Environments (MEaSUREs) program. QY, EJF,
MS, SW, and BHK acknowledge the support of the AIRS project at JPL. The
efforts of X. L. Huang and X. H. Chen were supported by NASA Grant
NNX14AJ50G awarded to the University of Michigan. AIRS data were
obtained through the Goddard Earth Services Data and Information
Services Center (http://daac.gsfc.nasa.gov/). MODIS data were obtained
through the Level-1 and Atmosphere Archive and Distribution System
(LAADS; http://ladsweb.nascom.nasa.gov/). The authors thank B. Soden, M.
Zelinka, and G. Stephens for useful feedback in the preparation of this
manuscript and the anonymous reviewers for comments on this study.
NR 58
TC 3
Z9 3
U1 2
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD MAR
PY 2016
VL 29
IS 6
BP 2023
EP 2040
DI 10.1175/JCLI-D-15-0257.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DL6YS
UT WOS:000375786600004
ER
PT J
AU Miller, KE
Eigenbrode, JL
Freissinet, C
Glavin, DP
Kotrc, B
Francois, P
Summons, RE
AF Miller, Kristen E.
Eigenbrode, Jennifer L.
Freissinet, Caroline
Glavin, Daniel P.
Kotrc, Benjamin
Francois, Pascaline
Summons, Roger E.
TI Potential precursor compounds for chlorohydrocarbons detected in Gale
Crater, Mars, by the SAM instrument suite on the Curiosity Rover
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE chlorohydrocarbon; Gale Grater; Mars; Curiosity; Sample Analysis on Mars
ID ORGANIC-MOLECULES; MARTIAN SOIL; BENZENE; SURFACE
AB The detection of chlorinated organic compounds in near-surface sedimentary rocks by the Sample Analysis at Mars (SAM) instrument suite aboard the Mars Science Laboratory Curiosity rover represents an important step toward characterizing habitable environments on Mars. However, this discovery also raises questions about the identity and source of their precursor compounds and the processes by which they become chlorinated. Here we present the results of analog experiments, conducted under conditions similar to SAM gas chromatography-mass spectrometry analyses, in which we pyrolyzed potential precursor compounds in the presence of various Cl salts and Fe oxides that have been identified in Martian sediments. While chloromethanes could not be unambiguously identified, 1,2-dichloropropane (1,2-DCP), which is one of the chlorinated compounds identified in SAM data, is formed from the chlorination of aliphatic precursors. Additionally, propanol produced more 1,2-DCP than nonfunctionalized aliphatics such as propane or hexanes. Chlorinated benzenes ranging from chlorobenzene to hexachlorobenzene were identified in experiments with benzene carboxylic acids but not with benzene or toluene. Lastly, the distribution of chlorinated benzenes depended on both the substrate species and the nature and concentration of the Cl salt. Ca and Mg perchlorate, both of which release O-2 in addition to Cl-2 and HCl upon pyrolysis, formed less chlorobenzene relative to the sum of all chlorinated benzenes than in experiments with ferric chloride. FeCl3, a Lewis acid, catalyzes chlorination but does not aid combustion. Accordingly, both the precursor chemistry and sample mineralogy exert important controls on the distribution of chlorinated organics.
C1 [Miller, Kristen E.; Kotrc, Benjamin; Summons, Roger E.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Eigenbrode, Jennifer L.; Freissinet, Caroline; Glavin, Daniel P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Francois, Pascaline] Univ Paris 07, CNRS, Lab Inter Univ Syst Atmospher LISA, Creteil, France.
[Francois, Pascaline] Univ Paris Est Creteil, Creteil, France.
RP Summons, RE (reprint author), MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM rsummons@mit.edu
RI Glavin, Daniel/D-6194-2012
OI Glavin, Daniel/0000-0001-7779-7765
FU NASA Astrobiology Institute [NNA13AA90A]; NASA ROSES MSL Participating
Scientist Program
FX This work was supported by the NASA ROSES MSL Participating Scientist
Program through a grant to RES. We thank MSL and SAM science teams for
their helpful input. B. Kotrc received additional support from the NASA
Astrobiology Institute (NNA13AA90A). Data used for the results of this
paper are available upon request from the corresponding author
(rsummons@mit.edu). We thank Mildred Martin for technical assistance in
the work conducted at GSFC and Richard V Morris for the provision of the
magnetite used in our experiments. We thank the reviewers for their
comments and suggestions that aided us in improving the original
manuscript.
NR 29
TC 1
Z9 1
U1 13
U2 24
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR
PY 2016
VL 121
IS 3
BP 296
EP 308
DI 10.1002/2015JE004939
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DJ6VY
UT WOS:000374352500003
ER
PT J
AU Lasue, J
Clegg, SM
Forni, O
Cousin, A
Wiens, RC
Lanza, N
Mangold, N
Le Deit, L
Gasnault, O
Maurice, S
Berger, JA
Stack, K
Blaney, D
Fabre, C
Goetz, W
Johnson, J
Le Mouelic, S
Nachon, M
Payre, V
Rapin, W
Sumner, DY
AF Lasue, J.
Clegg, S. M.
Forni, O.
Cousin, A.
Wiens, R. C.
Lanza, N.
Mangold, N.
Le Deit, L.
Gasnault, O.
Maurice, S.
Berger, J. A.
Stack, K.
Blaney, D.
Fabre, C.
Goetz, W.
Johnson, J.
Le Mouelic, S.
Nachon, M.
Payre, V.
Rapin, W.
Sumner, D. Y.
TI Observation of > 5wt % zinc at the Kimberley outcrop, Gale crater, Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars; data reduction technique; laser-induced breakdown spectroscopy
(LIBS)
ID SCIENCE LABORATORY MISSION; CHEMCAM INSTRUMENT SUITE; CONTINENTAL-CRUST;
MINERALOGY; ROCKS; ROVER; GEOCHEMISTRY; EVOLUTION; DEPOSIT; ORIGIN
AB Zinc-enriched targets have been detected at the Kimberley formation, Gale crater, Mars, using the Chemistry Camera (ChemCam) instrument. The Zn content is analyzed with a univariate calibration based on the 481.2nm emission line. The limit of quantification for ZnO is 3wt % (at 95% confidence level) and 1wt % (at 68% confidence level). The limit of detection is shown to be around 0.5wt %. As of sol 950, 12 targets on Mars present high ZnO content ranging from 1.0wt % to 8.4wt % (Yarrada, sol 628). Those Zn-enriched targets are almost entirely located at the Dillinger member of the Kimberley formation, where high Mn and alkali contents were also detected, probably in different phases. Zn enrichment does not depend on the textures of the rocks (coarse-grained sandstones, pebbly conglomerates, and resistant fins). The lack of sulfur enhancement suggests that Zn is not present in the sphalerite phase. Zn appears somewhat correlated with Na2O and the ChemCam hydration index, suggesting that it could be in an amorphous clay phase (such as sauconite). On Earth, such an enrichment would be consistent with a supergene alteration of a sphalerite gossan cap in a primary siliciclastic bedrock or a possible hypogene nonsulfide zinc deposition where Zn, Fe, Mn would have been transported in a reduced sulfur-poor fluid and precipitated rapidly in the form of oxides.
C1 [Lasue, J.; Forni, O.; Cousin, A.; Gasnault, O.; Maurice, S.; Rapin, W.] CNRS, OMP, IRAP, Toulouse, France.
[Lasue, J.; Forni, O.; Cousin, A.; Gasnault, O.; Maurice, S.; Rapin, W.] UPS, OMP, IRAP, Toulouse, France.
[Clegg, S. M.] Los Alamos Natl Lab, C PCS, MS J565, Los Alamos, NM USA.
[Wiens, R. C.; Lanza, N.; Le Mouelic, S.; Nachon, M.] Los Alamos Natl Lab, ISR, MS D466, Los Alamos, NM USA.
[Mangold, N.; Le Deit, L.; Le Mouelic, S.; Nachon, M.] Los Alamos Natl Lab, CNRS UMR 6112, LPGNantes, Lab Planetol & Geodynam, POB 1663, Los Alamos, NM USA.
[Berger, J. A.; Payre, V.] Univ Western Ontario, Dept Earth Sci, London, ON, Canada.
[Stack, K.; Blaney, D.; Sumner, D. Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Fabre, C.] Lorraine Univ, CNRS, GeoRessources, Vandoeuvre Les Nancy, France.
[Goetz, W.] Max Planck Inst Stromungsforsch, Bunsenstr 10, D-37073 Gottingen, Germany.
[Johnson, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Lasue, J (reprint author), CNRS, OMP, IRAP, Toulouse, France.; Lasue, J (reprint author), UPS, OMP, IRAP, Toulouse, France.
EM jlasue@irap.omp.eu
RI Gasnault, Olivier/F-4327-2010;
OI Gasnault, Olivier/0000-0002-6979-9012; Clegg, Sam/0000-0002-0338-0948
FU NASA Mars Exploration Program; CNES; CNRS
FX The authors acknowledge fruitful discussions with Ralf Gellert. We are
grateful to C.A. Johnson, P. Giesting, and M. Boni for very constructive
and useful comments which helped significantly improve the manuscript.
Funding for MSL and ChemCam operations and science in the U.S. was
provided by the NASA Mars Exploration Program. Funding for ChemCam
operations in France was provided by CNES; science funding in France was
provided by CNRS. The authors gratefully acknowledge the support of all
of the people at JPL involved in making MSL a successful mission. The
data used in this study were generated by the ChemCam and the Mars
Science Laboratory teams and are freely available at the Planetary Data
Systemof NASA (https://pds.jpl.nasa.gov/). All data described in the
text are indicated together with the spacecraft clock and three letters
that describe the type of data used, which singly identify the data in
PDS.
NR 62
TC 5
Z9 5
U1 4
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR
PY 2016
VL 121
IS 3
BP 338
EP 352
DI 10.1002/2015JE004946
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DJ6VY
UT WOS:000374352500005
ER
PT J
AU Mangold, N
Thompson, LM
Forni, O
Williams, AJ
Fabre, C
Le Deit, L
Wiens, RC
Williams, R
Anderson, RB
Blaney, DL
Calef, F
Cousin, A
Clegg, SM
Dromart, G
Dietrich, WE
Edgett, KS
Fisk, MR
Gasnault, O
Gellert, R
Grotzinger, JP
Kah, L
Le Mouelic, S
McLennan, SM
Maurice, S
Meslin, PY
Newsom, HE
Palucis, MC
Rapin, W
Sautter, V
Siebach, KL
Stack, K
Sumner, D
Yingst, A
AF Mangold, N.
Thompson, L. M.
Forni, O.
Williams, A. J.
Fabre, C.
Le Deit, L.
Wiens, R. C.
Williams, R.
Anderson, R. B.
Blaney, D. L.
Calef, F.
Cousin, A.
Clegg, S. M.
Dromart, G.
Dietrich, W. E.
Edgett, K. S.
Fisk, M. R.
Gasnault, O.
Gellert, R.
Grotzinger, J. P.
Kah, L.
Le Mouelic, S.
McLennan, S. M.
Maurice, S.
Meslin, P-Y.
Newsom, H. E.
Palucis, M. C.
Rapin, W.
Sautter, V.
Siebach, K. L.
Stack, K.
Sumner, D.
Yingst, A.
TI Composition of conglomerates analyzed by the Curiosity rover:
Implications for Gale Crater crust and sediment sources
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars; fluvial; sedimentary rocks; Gale Crater
ID CHEMCAM INSTRUMENT SUITE; CONTINENTAL-CRUST; YELLOWKNIFE BAY; MARTIAN
CRUST; GRAIN-SIZE; MARS; EVOLUTION; DIVERSITY; METEORITE; OLIVINE
AB The Curiosity rover has analyzed various detrital sedimentary rocks at Gale Crater, among which fluvial and lacustrine rocks are predominant. Conglomerates correspond both to the coarsest sediments analyzed and the least modified by chemical alteration, enabling us to link their chemistry to that of source rocks on the Gale Crater rims. In this study, we report the results of six conglomerate targets analyzed by Alpha-Particle X-ray Spectrometer and 40 analyzed by ChemCam. The bulk chemistry derived by both instruments suggests two distinct end-members for the conglomerate compositions. The first group (Darwin type) is typical of conglomerates analyzed before sol 540; it has a felsic alkali-rich composition, with a Na2O/K2O>5. The second group (Kimberley type) is typical of conglomerates analyzed between sols 540 and 670 in the vicinity of the Kimberley waypoint; it has an alkali-rich potassic composition with Na2O/K2O<2. The variety of chemistry and igneous textures (when identifiable) of individual clasts suggest that each conglomerate type is a mixture of multiple source rocks. Conglomerate compositions are in agreement with most of the felsic alkali-rich float rock compositions analyzed in the hummocky plains. The average composition of conglomerates can be taken as a proxy of the average igneous crust composition at Gale Crater. Differences between the composition of conglomerates and that of finer-grained detrital sediments analyzed by the rover suggest modifications by diagenetic processes (especially for Mg enrichments in fine-grained rocks), physical sorting, and mixing with finer-grained material of different composition.
C1 [Mangold, N.; Le Deit, L.; Le Mouelic, S.] Univ Nantes, CNRS, Lab Planetol & Geodynam Nantes, UMR 6112, Nantes, France.
[Thompson, L. M.] Univ New Brunswick, Dept Earth Sci, Planetary & Space Sci Ctr, Fredericton, NB, Canada.
[Forni, O.; Cousin, A.; Gasnault, O.; Maurice, S.; Meslin, P-Y.; Rapin, W.] Univ Toulouse, UPS OMP, CNRS, Inst Rech Astrophys & Planetol, Toulouse, France.
[Williams, A. J.] Towson Univ, Dept Phys Astron & Geosci, Towson, MD USA.
[Fabre, C.] Univ Lorraine, GeoRessources, Nancy, France.
[Wiens, R. C.; Clegg, S. M.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Williams, R.; Yingst, A.] Planetary Sci Inst, Tucson, AZ USA.
[Anderson, R. B.] USGS, Flagstaff, AZ USA.
[Blaney, D. L.; Calef, F.; Stack, K.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Dromart, G.] Univ Lyon, Lab Geol Lyon, Lyon, France.
[Dietrich, W. E.; Palucis, M. C.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Edgett, K. S.] Malin Space Sci Syst, San Diego, CA USA.
[Fisk, M. R.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR USA.
[Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada.
[Grotzinger, J. P.; Siebach, K. L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Kah, L.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA.
[McLennan, S. M.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA.
[Newsom, H. E.] Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Sautter, V.] Museum Natl Hist Nat, IMPMC, F-75231 Paris, France.
[Sumner, D.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA.
RP Mangold, N (reprint author), Univ Nantes, CNRS, Lab Planetol & Geodynam Nantes, UMR 6112, Nantes, France.
EM nicolas.mangold@univ-nantes.fr
RI Gasnault, Olivier/F-4327-2010;
OI Gasnault, Olivier/0000-0002-6979-9012; Siebach,
Kirsten/0000-0002-6628-6297; Clegg, Sam/0000-0002-0338-0948
FU French space agency, Centre National d'Etudes Spatiales (CNES); Canadian
Space Agency (CSA)
FX We are grateful to Marjorie Chan and two anonymous reviewers for their
insightful comments. Development and operation of the ChemCam instrument
was supported in France by funds from the French space agency, Centre
National d'Etudes Spatiales (CNES). Support for development and
operation in the U.S. was provided by NASA to the Mars Exploration
Program and specifically to the MSL team. The APXS is managed and
financed by the Canadian Space Agency (CSA). Imaging and chemical data
presented here are available in the NASA Planetary Data System (PDS)
http://pds-geosciences.wustl.edu/missions/msl. We are grateful to the
MSL engineering and management teams (and especially the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA) for making the mission and this scientific investigation possible
and to science team members who contributed to mission operations.
NR 96
TC 4
Z9 4
U1 7
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR
PY 2016
VL 121
IS 3
BP 353
EP 387
DI 10.1002/2015JE004977
PG 35
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DJ6VY
UT WOS:000374352500006
ER
PT J
AU Palucis, MC
Dietrich, WE
Williams, RME
Hayes, AG
Parker, T
Sumner, DY
Mangold, N
Lewis, K
Newsom, H
AF Palucis, Marisa C.
Dietrich, William E.
Williams, Rebecca M. E.
Hayes, Alexander G.
Parker, Tim
Sumner, Dawn Y.
Mangold, Nicolas
Lewis, Kevin
Newsom, Horton
TI Sequence and relative timing of large lakes in Gale crater (Mars) after
the formation of Mount Sharp
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Gale; Mars; Mars Science Laboratory; paleolakes; deltas; fans
ID LIQUID WATER; ASTRONOMICAL THEORY; SEDIMENTARY-ROCKS; FLUVIAL ACTIVITY;
ALLUVIAL FANS; EVOLUTION; ORIGIN; ICE; CONSTRAINTS; EVAPORATION
AB The quantification of lake levels in Gale crater is important to define the hydrologic and climatic history experienced by the sedimentary deposits found by Curiosity. We propose that there were at least three major lake stands within Gale, each persisted >1000years, and all occurred after Mount Sharp reached close to its current topographic form. Deltaic deposits off the southern rim of Gale, derived from incision of Farah Vallis, and corresponding deposits off the southern flank of Mount Sharp define the highest lake level, which had a mean depth of 700m. Canyons similar in form to Farah Vallis enter into craters and/or the crustal dichotomy near Gale from the south, suggesting that the highest lake was supplied by a large-scale flow system. The next lake level, established after a period of drying and rewetting, is defined by four deltaic features, three sourced from Mount Sharp and one from the western rim of Gale, as well as the termination of gullies around the northern rim of Gale. This second lake level had a mean depth of 300m. The presence of the gullies suggests more locally sourced water. Lake levels then rose another 100m, as evidenced by two deltaic deposits derived from the rim of Gale and the termination of a second set of gullies. Post-lake, reduced hydrologic activity continued, evidenced by a time of fan building (including Peace Vallis). The sequence of events suggests an episodic shift through time from relatively wet regional conditions to a drier environment with local runoff.
C1 [Palucis, Marisa C.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Dietrich, William E.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Williams, Rebecca M. E.] Planetary Sci Inst, Tucson, AZ USA.
[Hayes, Alexander G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Parker, Tim] NASA, Jet Prop Lab, CALTECH, Pasadena, CA 91125 USA.
[Sumner, Dawn Y.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA.
[Mangold, Nicolas] Univ Nantes, CNRS UMR6112, LPGN, Nantes, France.
[Lewis, Kevin] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Newsom, Horton] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
RP Palucis, MC (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM mpalucis@caltech.edu
NR 69
TC 2
Z9 2
U1 8
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR
PY 2016
VL 121
IS 3
BP 472
EP 496
DI 10.1002/2015JE004905
PG 25
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DJ6VY
UT WOS:000374352500011
ER
PT J
AU Yant, M
Rogers, AD
Nekvasil, H
Zhao, YYS
Bristow, T
AF Yant, Marcella
Rogers, A. Deanne
Nekvasil, Hanna
Zhao, Yu-Yan Sara
Bristow, Tom
TI Spectral characterization of acid weathering products on Martian
basaltic glass
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE infrared; geochemistry; Mars; weathering; acid; sulfates
ID THERMAL EMISSION SPECTROMETER; INFRARED REFLECTANCE SPECTROSCOPY;
OMEGA/MARS EXPRESS; MERIDIANI-PLANUM; CRYSTALLINE HEMATITE; SULFATE
ALTERATION; KILAUEA VOLCANO; GUSEV CRATER; GLOBAL VIEW; EARLY MARS
AB For the first time, direct infrared spectral analyses of glasses with Martian compositions, altered under controlled conditions, are presented in order to assess surface weathering and regolith development on Mars. Basaltic glasses of Irvine and Backstay composition were synthesized and altered using H2SO4-HCl acid solutions (pH0-4). Scanning electron microscopy/energy dispersive spectroscopy, X-ray diffraction, Raman, and infrared spectral measurements were acquired for each reaction product. Infrared spectra were also acquired from previously synthesized and altered glasses with Pathfinder-measured compositions. Acid alteration on particles in the most acidic solutions (pH1) yielded sulfate-dominated visible near infrared (VNIR) and thermal infrared (TIR) spectra with some silica influence. Spectral differences between alteration products from each starting material were present, reflecting strong sensitivity to changes in mineral assemblage. In the TIR, alteration features were preserved after reworking and consolidation. In the VNIR, hydrated sulfate features were present along with strong negative spectral slopes. Although such signatures are found in a few isolated locations on Mars with high-resolution spectrometers, much of the Martian surface lacks these characteristics, suggesting the following: acid alteration occurred at pH2; small amounts of sulfates were reworked with unaltered material; there is a prevalence of intermediate-to-high silica glass in Martian starting materials (more resistant to acid alteration); primary or added sulfur were lacking; alteration features are obscured by dust; and/or large-scale, pervasive, acid sulfate weathering of the Martian surface did not occur. These results highlight the need to better understand the spectral properties of altered Martian surface material in order to enhance the interpretation of remote spectra for altered terrains.
C1 [Yant, Marcella; Rogers, A. Deanne; Nekvasil, Hanna; Zhao, Yu-Yan Sara] SUNY Stony Brook, Dept Geosci, New York, NY USA.
[Bristow, Tom] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA USA.
RP Yant, M (reprint author), SUNY Stony Brook, Dept Geosci, New York, NY USA.
EM Marcella.Yant@stonybrook.edu
RI Rogers, Deanne/I-9737-2016
OI Rogers, Deanne/0000-0002-4671-2551
FU NASA [NNX13AP67G]
FX This work was funded by NASA grant NNX13AP67G to A.D.R. All infrared and
Raman spectra presented in this work were acquired at the Stony Brook
University Vibrational Spectroscopy Laboratory. The authors would like
to thank Don Lindsley for helpful discussions, James Quinn for
assistance with SEM, and Nick Tosca for donating the altered Pathfinder
samples. We also would like to thank the two anonymous reviewers for
their very helpful comments. Supporting data are included as three
tables in a supporting information file; any additional data may be
obtained from Marcella Yant (email: Marcella.Yant@stonybrook.edu).
NR 91
TC 2
Z9 2
U1 5
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAR
PY 2016
VL 121
IS 3
BP 516
EP 541
DI 10.1002/2015JE004969
PG 26
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DJ6VY
UT WOS:000374352500013
ER
PT J
AU Jetz, W
Cavender-Bares, J
Pavlick, R
Schimel, D
Davis, FW
Asner, GP
Guralnick, R
Kattge, J
Latimer, AM
Moorcroft, P
Schaepman, ME
Schildhauer, MP
Schneider, FD
Schrodt, F
Stahl, U
Ustin, SL
AF Jetz, Walter
Cavender-Bares, Jeannine
Pavlick, Ryan
Schimel, David
Davis, Frank W.
Asner, Gregory P.
Guralnick, Robert
Kattge, Jens
Latimer, Andrew M.
Moorcroft, Paul
Schaepman, Michael E.
Schildhauer, Mark P.
Schneider, Fabian D.
Schrodt, Franziska
Stahl, Ulrike
Ustin, Susan L.
TI Monitoring plant functional diversity from space
SO NATURE PLANTS
LA English
DT Editorial Material
ID IMAGING SPECTROSCOPY; ECOSYSTEM SERVICES; TERRESTRIAL ECOSYSTEMS; LITTER
DECOMPOSITION; FOREST ECOSYSTEMS; LEAF-AREA; BIODIVERSITY; NITROGEN;
TRAITS; LIGNIN
C1 [Jetz, Walter] Yale Univ, 165 Prospect St, New Haven, CT 06520 USA.
[Cavender-Bares, Jeannine] Univ Minnesota, Dept Ecol Evolut & Behav, 1987 Upper Buford Circle, St Paul, MN 55108 USA.
[Pavlick, Ryan; Schimel, David] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Davis, Frank W.; Schildhauer, Mark P.] Univ Calif Santa Barbara, Natl Ctr Ecol Anal & Synth, 735 State St,Suite 300, Santa Barbara, CA 93101 USA.
[Asner, Gregory P.] Carnegie Inst Sci, Dept Global Ecol, 290 Panama St, Stanford, CA 94305 USA.
[Guralnick, Robert] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Kattge, Jens; Stahl, Ulrike] Max Planck Inst Biogeochem, Hans Knoll Str 10, D-07745 Jena, Germany.
[Latimer, Andrew M.] Univ Calif Davis, Dept Plant Sci, 139 Veihmeyer Hall, Davis, CA 95616 USA.
[Moorcroft, Paul] Harvard Univ, 26 Oxford St,HMNH,Suite 43, Cambridge, MA 02138 USA.
[Schaepman, Michael E.; Schneider, Fabian D.] Univ Zurich, Winterthurerstr 190, CH-8057 Zurich, Switzerland.
[Schrodt, Franziska] Univ Brighton, Sch Geog, 9 Old Court Close, Brighton BN1 8HF, E Sussex, England.
[Ustin, Susan L.] Univ Calif Davis, Ctr Spatial Technol & Remote Sensing, 139 Veihmeyer Hall, Davis, CA 95616 USA.
RP Jetz, W (reprint author), Yale Univ, 165 Prospect St, New Haven, CT 06520 USA.; Cavender-Bares, J (reprint author), Univ Minnesota, Dept Ecol Evolut & Behav, 1987 Upper Buford Circle, St Paul, MN 55108 USA.
EM walter.jetz@yale.edu; cavender@umn.edu
RI Kattge, Jens/J-8283-2016; Schaepman, Michael/B-9213-2009; Davis,
Frank/B-7010-2009; Schrodt, Franziska/D-2260-2017;
OI Kattge, Jens/0000-0002-1022-8469; Schaepman,
Michael/0000-0002-9627-9565; Davis, Frank/0000-0002-4643-5718; Schrodt,
Franziska/0000-0001-9053-8872; Schildhauer, Mark/0000-0003-0632-7576
NR 84
TC 11
Z9 11
U1 20
U2 46
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2055-026X
EI 2055-0278
J9 NAT PLANTS
JI Nat. Plants
PD MAR
PY 2016
VL 2
IS 3
AR 16024
DI 10.1038/NPLANTS.2016.24
PG 5
WC Plant Sciences
SC Plant Sciences
GA DL1MA
UT WOS:000375395000006
PM 27249357
ER
PT J
AU Solander, KC
Reager, JT
Famiglietti, JS
AF Solander, Kurt C.
Reager, John T.
Famiglietti, James S.
TI How well will the Surface Water and Ocean Topography (SWOT) mission
observe global reservoirs?
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE remote sensing; reservoirs; global observations; SWOT
ID STORAGE CHANGES; MANAGEMENT; DISCHARGE; LAKES
AB Accurate observations of global reservoir storage are critical to understand the availability of managed water resources. By enabling estimates of surface water area and height for reservoir sizes exceeding 250 m(2) at a maximum repeat orbit of up to 21 days, the NASA Surface Water and Ocean Topography (SWOT) satellite mission (anticipated launch date 2020) is expected to greatly improve upon existing reservoir monitoring capabilities. It is thus essential that spatial and temporal measurement uncertainty for water bodies is known a priori to maximize the utility of SWOT observations as the data are acquired. In this study, we evaluate SWOT reservoir observations using a three-pronged approach that assesses temporal aliasing, errors due to specific reservoir spatial properties, and SWOT performance over actual reservoirs using a combination of in situ and simulated reservoir observations from the SWOTsim instrument simulator. Results indicate temporal errors to be less than 5% for the smallest reservoir sizes (< 10 km(2)) with errors less than 0.1% for larger sizes (>100 km(2)). Surface area and height errors were found to be minimal (area <5%, height <15 cm) above 1 km(2) unless the reservoir exhibited a strong elliptical shape with high aspect ratio oriented parallel to orbit, was set in mountainous terrain, or swath coverage fell below 30%. Experiments from six real reservoir test cases generally support these results. By providing a comprehensive blueprint on the observability of reservoirs from SWOT, this study will be have important implications for future applications of SWOT reservoir measurements in global monitoring systems and models.
C1 [Solander, Kurt C.; Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Reager, John T.; Famiglietti, James S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA USA.
RP Famiglietti, JS (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.; Famiglietti, JS (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.; Famiglietti, JS (reprint author), Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA USA.
EM James.Famiglietti@nasa.jpl.gov
FU National Aeronautics and Space Administration (NASA) Earth and Space
Science Fellowship (NESSF); Jet Propulsion Laboratory, California
Institute of Technology; NASA
FX The SWOTsim instrument simulator (v2, acquired 1 October 2014) provided
much of the data that were used in this study and is under ongoing
development. A portion of this work was conducted at the Jet Propulsion
Laboratory, California Institute of Technology (JPL-Cal Tech), under
contract with NASA. In situ data were obtained from the California
Department of Water Resources California Data Exchange Center
(www.cdec.water.ca.gov, accessed 18 August 2014). Digital Elevation
Model (DEM) data used in this study came from the NASA ASTER GDEM v2 at
30 m resolution (http://gdex.cr.usgs.gov/gdex/, accessed 5 December
2014). The authors are particularly grateful for the generous financial
support received from the National Aeronautics and Space Administration
(NASA) Earth and Space Science Fellowship (NESSF) for this research. We
would also like to thank members of the SWOT Science Definition Team, in
particular Konstantios M. Andreadis and Brent A. Williams for providing
assistance and information on the SWOTsim instrument simulator. The
authors John T. Reager and James S. Famiglietti were partially supported
by the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with NASA.
NR 31
TC 0
Z9 0
U1 3
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD MAR
PY 2016
VL 52
IS 3
BP 2123
EP 2140
DI 10.1002/2015WR017952
PG 18
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA DK1WR
UT WOS:000374706300031
ER
PT J
AU Espinoza-Davalos, GE
Arctur, DK
Teng, W
Maidment, DR
Garcia-Marti, I
Comair, G
AF Espinoza-Davalos, Gonzalo E.
Arctur, David K.
Teng, William
Maidment, David R.
Garcia-Marti, Irene
Comair, Georges
TI Studying soil moisture at a national level through statistical analysis
of NASA NLDAS data
SO JOURNAL OF HYDROINFORMATICS
LA English
DT Article
DE cloud processing; data rods; NLDAS; soil moisture; web services; web
applications
ID RAINFALL; PREDICTION; EXTREMES; SUPPORT; MODEL
AB The purpose of this research is to enable better understanding of current environmental conditions through the relations of environmental variables to the historical record. Our approach is to organize and visualize land surface model (LSM) outputs and statistics in a web application, using the latest technologies in geographic information systems (GISs), web services, and cloud computing. The North American Land Data Assimilation System (NLDAS-2) (http://ldas.gsfc.nasa.gov/nldas/; Documentation: ftp://hydro1.sci.gsfc.nasa.gov/data/s4pa/NLDAS/README.NLDAS2.pdf) drives four LSM (e.g., Noah) (http://ldas.gsfc.nasa.gov/nldas/NLDAS2model.php) that simulate a suite of states and fluxes for central North America. The NLDAS-2 model output is accessible via multiple methods, designed to handle the outputs as time-step arrays. To facilitate data access as time series, selected NLDAS-Noah variables have been replicated by NASA as point-location files. These time series files or 'data rods' are accessible through web services. In this research, 35-year historical daily cumulative distribution functions (CDFs) are constructed using the data rods for the top-meter soil moisture variable. The statistical data are stored in and served from the cloud. The latest values in the Noah model are compared with the CDFs and displayed in a web application. Two case studies illustrate the utility of this approach: the 2011 Texas drought, and the 31 October 2013 flash flood in Austin, Texas.
C1 [Espinoza-Davalos, Gonzalo E.; Arctur, David K.; Maidment, David R.] Univ Texas Austin, Austin, TX 78712 USA.
[Teng, William] NASA, Goddard Earth Sci Data & Informat Serv Ctr, Greenbelt, MD USA.
[Garcia-Marti, Irene] Univ Twente, Drienerlolaan 5, NL-7522 NB Enschede, Netherlands.
[Comair, Georges] Suez Environm, Paris, France.
RP Espinoza-Davalos, GE (reprint author), Univ Texas Austin, Austin, TX 78712 USA.
EM gespinoza@utexas.edu
OI Espinoza-Davalos, Gonzalo/0000-0002-8137-7525
FU NASA under the ROSES-ACCESS project [NNH11ZDA001N]
FX The research was funded by NASA under the ROSES NNH11ZDA001N-ACCESS
project. The authors gratefully acknowledge the Texas Advanced Computing
Center (TACC) at The University of Texas at Austin for providing HPC
resources that have contributed to the research results reported within
this paper (http://www.tacc.utexas.edu).
NR 28
TC 2
Z9 2
U1 3
U2 5
PU IWA PUBLISHING
PI LONDON
PA ALLIANCE HOUSE, 12 CAXTON ST, LONDON SW1H0QS, ENGLAND
SN 1464-7141
EI 1465-1734
J9 J HYDROINFORM
JI J. Hydroinform.
PD MAR
PY 2016
VL 18
IS 2
BP 277
EP 287
DI 10.2166/hydro.2015.231
PG 11
WC Computer Science, Interdisciplinary Applications; Engineering, Civil;
Environmental Sciences; Water Resources
SC Computer Science; Engineering; Environmental Sciences & Ecology; Water
Resources
GA DJ6JJ
UT WOS:000374317600010
ER
PT J
AU Burch, JL
Moore, TE
Torbert, RB
Giles, BL
AF Burch, J. L.
Moore, T. E.
Torbert, R. B.
Giles, B. L.
TI Magnetospheric Multiscale Overview and Science Objectives
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Magnetic reconnection; Space plasma physics
ID MAGNETIC RECONNECTION; LABORATORY PLASMAS; ENERGY-CONVERSION; FIELD;
ION; MAGNETOPAUSE; MAGNETOTAIL; SPACE; WIND
AB Magnetospheric Multiscale (MMS), a NASA four-spacecraft constellation mission launched on March 12, 2015, will investigate magnetic reconnection in the boundary regions of the Earth's magnetosphere, particularly along its dayside boundary with the solar wind and the neutral sheet in the magnetic tail. The most important goal of MMS is to conduct a definitive experiment to determine what causes magnetic field lines to reconnect in a collisionless plasma. The significance of the MMS results will extend far beyond the Earth's magnetosphere because reconnection is known to occur in interplanetary space and in the solar corona where it is responsible for solar flares and the disconnection events known as coronal mass ejections. Active research is also being conducted on reconnection in the laboratory and specifically in magnetic-confinement fusion devices in which it is a limiting factor in achieving and maintaining electron temperatures high enough to initiate fusion. Finally, reconnection is proposed as the cause of numerous phenomena throughout the universe such as comet-tail disconnection events, magnetar flares, supernova ejections, and dynamics of neutron-star accretion disks. The MMS mission design is focused on answering specific questions about reconnection at the Earth's magnetosphere. The prime focus of the mission is on determining the kinetic processes occurring in the electron diffusion region that are responsible for reconnection and that determine how it is initiated; but the mission will also place that physics into the context of the broad spectrum of physical processes associated with reconnection. Connections to other disciplines such as solar physics, astrophysics, and laboratory plasma physics are expected to be made through theory and modeling as informed by the MMS results.
C1 [Burch, J. L.] SW Res Inst, San Antonio, TX USA.
[Moore, T. E.; Giles, B. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Torbert, R. B.] Univ New Hampshire, Durham, NH 03824 USA.
[Torbert, R. B.] SW Res Inst, Durham, NH USA.
RP Burch, JL (reprint author), SW Res Inst, San Antonio, TX USA.
EM jburch@swri.edu
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NASA [NNG04EB99C]
FX The dedicated efforts of the entire MMS team are greatly appreciated. We
are especially grateful to the leadership of the GSFC Project Manager,
Craig Tooley, his Deputy, Brent Robertson, and the SwRI SMART Project
Manager, Ron Black. This work was supported by NASA Contract No.
NNG04EB99C at SwRI.
NR 68
TC 103
Z9 104
U1 12
U2 18
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2016
VL 199
IS 1-4
BP 5
EP 21
DI 10.1007/s11214-015-0164-9
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6DI
UT WOS:000374299800002
ER
PT J
AU Tooley, CR
Black, RK
Robertson, BP
Stone, JM
Pope, SE
Davis, GT
AF Tooley, C. R.
Black, R. K.
Robertson, B. P.
Stone, J. M.
Pope, S. E.
Davis, G. T.
TI The Magnetospheric Multiscale Constellation
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Magnetospheric multiscale; Magnetic reconnection; Space mission design;
Spacecraft design; GPS; Formation flying; Spinning spacecraft
AB The Magnetospheric Multiscale (MMS) mission is the fourth mission of the Solar Terrestrial Probe (STP) program of the National Aeronautics and Space Administration (NASA). The MMS mission was launched on March 12, 2015. The MMS mission consists of four identically instrumented spin-stabilized observatories which are flown in formation to perform the first definitive study of magnetic reconnection in space. The MMS mission was presented with numerous technical challenges, including the simultaneous construction and launch of four identical large spacecraft with 100 instruments total, stringent electromagnetic cleanliness requirements, closed-loop precision maneuvering and pointing of spinning flexible spacecraft, on-board GPS based orbit determination far above the GPS constellation, and a flight dynamics design that enables formation flying with separation distances as small as 10 km. This paper describes the overall mission design and presents an overview of the design, testing, and early on-orbit operation of the spacecraft systems and instrument suite.
C1 [Tooley, C. R.; Robertson, B. P.; Davis, G. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Black, R. K.; Stone, J. M.; Pope, S. E.] SW Res Inst, San Antonio, TX USA.
RP Tooley, CR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM craig.r.tooley@nasa.gov
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
NR 19
TC 1
Z9 1
U1 2
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2016
VL 199
IS 1-4
BP 23
EP 76
DI 10.1007/s11214-015-0220-5
PG 54
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6DI
UT WOS:000374299800003
ER
PT J
AU Fuselier, SA
Lewis, WS
Schiff, C
Ergun, R
Burch, JL
Petrinec, SM
Trattner, KJ
AF Fuselier, S. A.
Lewis, W. S.
Schiff, C.
Ergun, R.
Burch, J. L.
Petrinec, S. M.
Trattner, K. J.
TI Magnetospheric Multiscale Science Mission Profile and Operations
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Magnetospheric multiscale; Magnetic reconnection; Space mission design;
Spacecraft orbits
ID SOLAR-WIND CONTROL; MAGNETIC RECONNECTION; MAGNETOPAUSE; MAGNETOTAIL;
LOCATION; MOTION; SHAPE; SITE
AB The Magnetospheric Multiscale (MMS) mission and operations are designed to provide the maximum reconnection science. The mission phases are chosen to investigate reconnection at the dayside magnetopause and in the magnetotail. At the dayside, the MMS orbits are chosen to maximize encounters with the magnetopause in regions where the probability of encountering the reconnection diffusion region is high. In the magnetotail, the orbits are chosen to maximize encounters with the neutral sheet, where reconnection is known to occur episodically. Although this targeting is limited by engineering constraints such as total available fuel, high science return orbits exist for launch dates over most of the year. The tetrahedral spacecraft formation has variable spacing to determine the optimum separations for the reconnection regions at the magnetopause and in the magnetotail. In the specific science regions of interest, the spacecraft are operated in a fast survey mode with continuous acquisition of burst mode data. Later, burst mode triggers and a ground-based scientist in the loop are used to determine the highest quality data to downlink for analysis. This operations scheme maximizes the science return for the mission.
C1 [Fuselier, S. A.; Lewis, W. S.; Burch, J. L.] SW Res Inst, San Antonio, TX USA.
[Fuselier, S. A.] Univ Texas San Antonio, San Antonio, TX 78249 USA.
[Schiff, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Ergun, R.; Trattner, K. J.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Petrinec, S. M.] Lockheed Martin STAR Labs, Palo Alto, CA 94304 USA.
RP Fuselier, SA (reprint author), SW Res Inst, San Antonio, TX USA.
EM sfuselier@swri.edu
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
NR 26
TC 19
Z9 19
U1 4
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2016
VL 199
IS 1-4
BP 77
EP 103
DI 10.1007/s11214-014-0087-x
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6DI
UT WOS:000374299800004
ER
PT J
AU Torbert, RB
Russell, CT
Magnes, W
Ergun, RE
Lindqvist, PA
LeContel, O
Vaith, H
Macri, J
Myers, S
Rau, D
Needell, J
King, B
Granoff, M
Chutter, M
Dors, I
Olsson, G
Khotyaintsev, YV
Eriksson, A
Kletzing, CA
Bounds, S
Anderson, B
Baumjohann, W
Steller, M
Bromund, K
Le, G
Nakamura, R
Strangeway, RJ
Leinweber, HK
Tucker, S
Westfall, J
Fischer, D
Plaschke, F
Porter, J
Lappalainen, K
AF Torbert, R. B.
Russell, C. T.
Magnes, W.
Ergun, R. E.
Lindqvist, P. -A.
LeContel, O.
Vaith, H.
Macri, J.
Myers, S.
Rau, D.
Needell, J.
King, B.
Granoff, M.
Chutter, M.
Dors, I.
Olsson, G.
Khotyaintsev, Y. V.
Eriksson, A.
Kletzing, C. A.
Bounds, S.
Anderson, B.
Baumjohann, W.
Steller, M.
Bromund, K.
Le, Guan
Nakamura, R.
Strangeway, R. J.
Leinweber, H. K.
Tucker, S.
Westfall, J.
Fischer, D.
Plaschke, F.
Porter, J.
Lappalainen, K.
TI The FIELDS Instrument Suite on MMS: Scientific Objectives, Measurements,
and Data Products
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Magnetic reconnection; Magnetospheric dynamics; Magnetospheric
multiscale; Electromagnetic field measurements
ID MAGNETIC-FIELD
AB The FIELDS instrumentation suite on the Magnetospheric Multiscale (MMS) mission provides comprehensive measurements of the full vector magnetic and electric fields in the reconnection regions investigated by MMS, including the dayside magnetopause and the night-side magnetotail acceleration regions out to 25 Re. Six sensors on each of the four MMS spacecraft provide overlapping measurements of these fields with sensitive cross-calibrations both before and after launch. The FIELDS magnetic sensors consist of redundant flux-gate magnetometers (AFG and DFG) over the frequency range from DC to 64 Hz, a search coil magnetometer (SCM) providing AC measurements over the full whistler mode spectrum expected to be seen on MMS, and an Electron Drift Instrument (EDI) that calibrates offsets for the magnetometers. The FIELDS three-axis electric field measurements are provided by two sets of biased double-probe sensors (SDP and ADP) operating in a highly symmetric spacecraft environment to reduce significantly electrostatic errors. These sensors are complemented with the EDI electric measurements that are free from all local spacecraft perturbations. Cross-calibrated vector electric field measurements are thus produced from DC to 100 kHz, well beyond the upper hybrid resonance whose frequency provides an accurate determination of the local electron density. Due to its very large geometric factor, EDI also provides very high time resolution (similar to 1 ms) ambient electron flux measurements at a few selected energies near 1 keV. This paper provides an overview of the FIELDS suite, its science objectives and measurement requirements, and its performance as verified in calibration and cross-calibration procedures that result in anticipated errors less than 0.1 nT in B and 0.5 mV/m in E. Summaries of data products that result from FIELDS are also described, as well as algorithms for cross-calibration. Details of the design and performance characteristics of AFG/DFG, SCM, ADP, SDP, and EDI are provided in five companion papers.
C1 [Torbert, R. B.; LeContel, O.; Vaith, H.; Macri, J.; Myers, S.; Rau, D.; Needell, J.; King, B.; Granoff, M.; Chutter, M.; Dors, I.] Univ New Hampshire, Durham, NH 03824 USA.
[Olsson, G.] Royal Inst Technol, Stockholm, Sweden.
[Khotyaintsev, Y. V.; Eriksson, A.] Swedish Inst Space Phys, Uppsala, Sweden.
[Porter, J.; Lappalainen, K.] Univ Oulu, Oulu, Finland.
[Ergun, R. E.; Tucker, S.; Westfall, J.] Univ Colorado, Boulder, CO 80309 USA.
[Torbert, R. B.] SW Res Inst, San Antonio, TX USA.
[Russell, C. T.; Strangeway, R. J.; Leinweber, H. K.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Bromund, K.; Le, Guan] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Kletzing, C. A.; Bounds, S.] Univ Iowa, Iowa City, IA USA.
[Anderson, B.] Johns Hopkins Appl Phys Lab, Laurel, MD USA.
[Magnes, W.; Baumjohann, W.; Steller, M.; Nakamura, R.; Fischer, D.; Plaschke, F.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
[Lindqvist, P. -A.] Plasma Phys Lab, Paris, France.
RP Torbert, RB (reprint author), Univ New Hampshire, Durham, NH 03824 USA.
EM roy.torbert@unh.edu
RI NASA MMS, Science Team/J-5393-2013; Nakamura, Rumi/I-7712-2013;
Baumjohann, Wolfgang/A-1012-2010; Le, Guan/C-9524-2012;
OI NASA MMS, Science Team/0000-0002-9504-5214; Nakamura,
Rumi/0000-0002-2620-9211; Baumjohann, Wolfgang/0000-0001-6271-0110; Le,
Guan/0000-0002-9504-5214; Kletzing, Craig/0000-0002-4136-3348
FU Space Science Center; EOS Institute at UNH; NASA MMS via the SwRI
[NNG04EB99C]
FX Development of the FIELDS instrumentation suite has been the joint
effort of many groups within the authors' institutions over the last 15
years. We acknowledge here generous support by the Space Science Center
and the EOS Institute at UNH and the many staff members who gave a great
part of their careers in the development of MMS. We wish to thank the
generous assistance of technical and management staff at NASA GSFC and
at SwRI, in particular W.C. Gibson and R.K. Black for managing the
entire SMART instrument suite. FIELDS was developed under NASA MMS
contract NNG04EB99C via the SwRI subcontract to UNH.
NR 20
TC 46
Z9 46
U1 3
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2016
VL 199
IS 1-4
BP 105
EP 135
DI 10.1007/s11214-014-0109-8
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6DI
UT WOS:000374299800005
ER
PT J
AU Russell, CT
Anderson, BJ
Baumjohann, W
Bromund, KR
Dearborn, D
Fischer, D
Le, G
Leinweber, HK
Leneman, D
Magnes, W
Means, JD
Moldwin, MB
Nakamura, R
Pierce, D
Plaschke, F
Rowe, KM
Slavin, JA
Strangeway, RJ
Torbert, R
Hagen, C
Jernej, I
Valavanoglou, A
Richter, I
AF Russell, C. T.
Anderson, B. J.
Baumjohann, W.
Bromund, K. R.
Dearborn, D.
Fischer, D.
Le, G.
Leinweber, H. K.
Leneman, D.
Magnes, W.
Means, J. D.
Moldwin, M. B.
Nakamura, R.
Pierce, D.
Plaschke, F.
Rowe, K. M.
Slavin, J. A.
Strangeway, R. J.
Torbert, R.
Hagen, C.
Jernej, I.
Valavanoglou, A.
Richter, I.
TI The Magnetospheric Multiscale Magnetometers
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Magnetosphere; Reconnection; Magnetometer
ID MAGNETIC-FIELD GRADIENTS; ACCURATE DETERMINATION; NATURAL CONSTRAINTS;
SPINNING SPACECRAFT; VECTOR MEASUREMENTS; SUBSTORMS; CLUSTER
AB The success of the Magnetospheric Multiscale mission depends on the accurate measurement of the magnetic field on all four spacecraft. To ensure this success, two independently designed and built fluxgate magnetometers were developed, avoiding single-point failures. The magnetometers were dubbed the digital fluxgate (DFG), which uses an ASIC implementation and was supplied by the Space Research Institute of the Austrian Academy of Sciences and the analogue magnetometer (AFG) with a more traditional circuit board design supplied by the University of California, Los Angeles. A stringent magnetic cleanliness program was executed under the supervision of the Johns Hopkins University's Applied Physics Laboratory. To achieve mission objectives, the calibration determined on the ground will be refined in space to ensure all eight magnetometers are precisely inter-calibrated. Near real-time data plays a key role in the transmission of high-resolution observations stored on board so rapid processing of the low-resolution data is required. This article describes these instruments, the magnetic cleanliness program, and the instrument pre-launch calibrations, the planned in-flight calibration program, and the information flow that provides the data on the rapid time scale needed for mission success.
C1 [Russell, C. T.; Dearborn, D.; Leinweber, H. K.; Leneman, D.; Means, J. D.; Rowe, K. M.; Strangeway, R. J.] Univ Calif Los Angeles, 603 Charles Young Dr, Los Angeles, CA 90095 USA.
[Anderson, B. J.] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
[Baumjohann, W.; Fischer, D.; Magnes, W.; Nakamura, R.; Plaschke, F.; Hagen, C.; Jernej, I.; Valavanoglou, A.] Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria.
[Bromund, K. R.; Le, G.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Moldwin, M. B.; Slavin, J. A.] Univ Michigan, 1032 Green St, Ann Arbor, MI 48109 USA.
[Pierce, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Torbert, R.] Univ New Hampshire, 105 Main St, Durham, NH 03824 USA.
[Richter, I.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, Mendelssohnstr 3, D-38106 Braunschweig, Germany.
RP Russell, CT (reprint author), Univ Calif Los Angeles, 603 Charles Young Dr, Los Angeles, CA 90095 USA.
EM ctrussell@igpp.ucla.edu
RI NASA MMS, Science Team/J-5393-2013; Nakamura, Rumi/I-7712-2013;
Baumjohann, Wolfgang/A-1012-2010; Le, Guan/C-9524-2012; Slavin,
James/H-3170-2012;
OI NASA MMS, Science Team/0000-0002-9504-5214; Nakamura,
Rumi/0000-0002-2620-9211; Baumjohann, Wolfgang/0000-0001-6271-0110; Le,
Guan/0000-0002-9504-5214; Slavin, James/0000-0002-9206-724X; Moldwin,
Mark/0000-0003-0954-1770
NR 22
TC 52
Z9 52
U1 5
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2016
VL 199
IS 1-4
BP 189
EP 256
DI 10.1007/s11214-014-0057-3
PG 68
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6DI
UT WOS:000374299800008
ER
PT J
AU Pollock, C
Moore, T
Jacques, A
Burch, J
Gliese, U
Saito, Y
Omoto, T
Avanov, L
Barrie, A
Coffey, V
Dorelli, J
Gershman, D
Giles, B
Rosnack, T
Salo, C
Yokota, S
Adrian, M
Aoustin, C
Auletti, C
Aung, S
Bigio, V
Cao, N
Chandler, M
Chornay, D
Christian, K
Clark, G
Collinson, G
Corris, T
De Los Santos, A
Devlin, R
Diaz, T
Dickerson, T
Dickson, C
Diekmann, A
Diggs, F
Duncan, C
Figueroa-Vinas, A
Firman, C
Freeman, M
Galassi, N
Garcia, K
Goodhart, G
Guererro, D
Hageman, J
Hanley, J
Hemminger, E
Holland, M
Hutchins, M
James, T
Jones, W
Kreisler, S
Kujawski, J
Lavu, V
Lobell, J
LeCompte, E
Lukemire, A
MacDonald, E
Mariano, A
Mukai, T
Narayanan, K
Nguyan, Q
Onizuka, M
Paterson, W
Persyn, S
Piepgrass, B
Cheney, F
Rager, A
Raghuram, T
Ramil, A
Reichenthal, L
Rodriguez, H
Rouzaud, J
Rucker, A
Saito, Y
Samara, M
Sauvaud, JA
Schuster, D
Shappirio, M
Shelton, K
Sher, D
Smith, D
Smith, K
Smith, S
Steinfeld, D
Szymkiewicz, R
Tanimoto, K
Taylor, J
Tucker, C
Tull, K
Uhl, A
Vloet, J
Walpole, P
Weidner, S
White, D
Winkert, G
Yeh, PS
Zeuch, M
AF Pollock, C.
Moore, T.
Jacques, A.
Burch, J.
Gliese, U.
Saito, Y.
Omoto, T.
Avanov, L.
Barrie, A.
Coffey, V.
Dorelli, J.
Gershman, D.
Giles, B.
Rosnack, T.
Salo, C.
Yokota, S.
Adrian, M.
Aoustin, C.
Auletti, C.
Aung, S.
Bigio, V.
Cao, N.
Chandler, M.
Chornay, D.
Christian, K.
Clark, G.
Collinson, G.
Corris, T.
De Los Santos, A.
Devlin, R.
Diaz, T.
Dickerson, T.
Dickson, C.
Diekmann, A.
Diggs, F.
Duncan, C.
Figueroa-Vinas, A.
Firman, C.
Freeman, M.
Galassi, N.
Garcia, K.
Goodhart, G.
Guererro, D.
Hageman, J.
Hanley, J.
Hemminger, E.
Holland, M.
Hutchins, M.
James, T.
Jones, W.
Kreisler, S.
Kujawski, J.
Lavu, V.
Lobell, J.
LeCompte, E.
Lukemire, A.
MacDonald, E.
Mariano, A.
Mukai, T.
Narayanan, K.
Nguyan, Q.
Onizuka, M.
Paterson, W.
Persyn, S.
Piepgrass, B.
Cheney, F.
Rager, A.
Raghuram, T.
Ramil, A.
Reichenthal, L.
Rodriguez, H.
Rouzaud, J.
Rucker, A.
Saito, Y.
Samara, M.
Sauvaud, J. -A.
Schuster, D.
Shappirio, M.
Shelton, K.
Sher, D.
Smith, D.
Smith, K.
Smith, S.
Steinfeld, D.
Szymkiewicz, R.
Tanimoto, K.
Taylor, J.
Tucker, C.
Tull, K.
Uhl, A.
Vloet, J.
Walpole, P.
Weidner, S.
White, D.
Winkert, G.
Yeh, P. -S.
Zeuch, M.
TI Fast Plasma Investigation for Magnetospheric Multiscale
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Magnetospheric Multiscale; Magnetic reconnection; Particle
instrumentation; Electron spectrometer; Ion spectrometer; Instrument
characterization and calibration
ID MICROCHANNEL PLATE; ION DETECTION; ELECTRON; SPACECRAFT; EFFICIENCY;
ANALYZER
AB The Fast Plasma Investigation (FPI) was developed for flight on the Magnetospheric Multiscale (MMS) mission to measure the differential directional flux of magnetospheric electrons and ions with unprecedented time resolution to resolve kinetic-scale plasma dynamics. This increased resolution has been accomplished by placing four dual 180-degree top hat spectrometers for electrons and four dual 180-degree top hat spectrometers for ions around the periphery of each of four MMS spacecraft. Using electrostatic field-of-view deflection, the eight spectrometers for each species together provide 4pi-sr field-of-view with, at worst, 11.25-degree sample spacing. Energy/charge sampling is provided by swept electrostatic energy/charge selection over the range from 10 eV/q to 30000 eV/q. The eight dual spectrometers on each spacecraft are controlled and interrogated by a single block redundant Instrument Data Processing Unit, which in turn interfaces to the observatory's Instrument Suite Central Instrument Data Processor. This paper describes the design of FPI, its ground and in-flight calibration, its operational concept, and its data products.
C1 [Pollock, C.; Moore, T.; Jacques, A.; Gliese, U.; Avanov, L.; Barrie, A.; Dorelli, J.; Gershman, D.; Giles, B.; Rosnack, T.; Salo, C.; Adrian, M.; Auletti, C.; Aung, S.; Bigio, V.; Cao, N.; Chornay, D.; Christian, K.; Clark, G.; Collinson, G.; Corris, T.; Devlin, R.; Dickerson, T.; Dickson, C.; Diggs, F.; Duncan, C.; Figueroa-Vinas, A.; Firman, C.; Galassi, N.; Garcia, K.; Hageman, J.; Hemminger, E.; Holland, M.; James, T.; Jones, W.; Kreisler, S.; Kujawski, J.; Lavu, V.; Lobell, J.; MacDonald, E.; Mariano, A.; Narayanan, K.; Nguyan, Q.; Onizuka, M.; Paterson, W.; Cheney, F.; Rager, A.; Raghuram, T.; Ramil, A.; Reichenthal, L.; Rucker, A.; Samara, M.; Schuster, D.; Shappirio, M.; Shelton, K.; Sher, D.; Smith, D.; Smith, S.; Steinfeld, D.; Szymkiewicz, R.; Tucker, C.; Tull, K.; Uhl, A.; Walpole, P.; Winkert, G.; Yeh, P. -S.; Zeuch, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Burch, J.; De Los Santos, A.; Diaz, T.; Freeman, M.; Goodhart, G.; Guererro, D.; Hanley, J.; Hutchins, M.; Persyn, S.; Piepgrass, B.; Rodriguez, H.; Smith, K.; Taylor, J.; Vloet, J.; Walpole, P.; Weidner, S.; White, D.] SW Res Inst, San Antonio, TX USA.
[Gliese, U.; Corris, T.; Devlin, R.; Galassi, N.; Uhl, A.] SGT Inc, Greenbelt, MD USA.
[Saito, Y.; Yokota, S.; Mukai, T.] Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229, Japan.
[Omoto, T.; Tanimoto, K.] Meisei Elect Co Ltd, Isesaki, Japan.
[Avanov, L.; Gershman, D.; Chornay, D.] Univ Maryland, College Pk, MD 20742 USA.
[Barrie, A.] Millenium Engn, Arlington, VA USA.
[Coffey, V.; Chandler, M.; Diekmann, A.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA.
[Gershman, D.] Oak Ridge Associated Univ, Oak Ridge, TN USA.
[Rosnack, T.; Aung, S.; Lavu, V.; Smith, D.] Orbital Sci Corp, Beltsville, MD USA.
[Salo, C.] Stellar Solut Inc, Chantilly, VA USA.
[Aoustin, C.; LeCompte, E.; Rouzaud, J.; Sauvaud, J. -A.] Inst Res Astrophys & Planetol, Toulouse, France.
[Auletti, C.; Dickson, C.; Diggs, F.; Rucker, A.; Zeuch, M.] Northrup Grumman, Hyattsville, MD USA.
[Auletti, C.] Florez Engn LLC, Laurel, MD USA.
[Cao, N.] MEI Technol, Houston, TX USA.
[Christian, K.] Global Programming Solut, Fairfax, VA USA.
[Clark, G.; Collinson, G.; Rager, A.; Smith, S.] Catholic Univ Amer, Washington, DC 20064 USA.
[Clark, G.] Johns Hopkins Appl Phys Lab, Laurel, MD USA.
[Dickerson, T.; Raghuram, T.; Shelton, K.] ASRC AS & D Inc, Beltsville, MD USA.
[Diekmann, A.] Jacobs ESSSA Grp, Huntsville, AL USA.
[Firman, C.] Prototype Prod Inc, Ashburn, VA USA.
[Hemminger, E.] Ares Tech Serv Corp, Greenbelt, MD USA.
[Jones, W.] Bandwidth Solut Inc, Mclean, VA USA.
[Kreisler, S.] Hammers Co, Greenbelt, MD USA.
[Kujawski, J.] Siena Coll, Loudonville, NY USA.
[Lukemire, A.] Space Power Elect Inc, Kathleen, GA USA.
[Onizuka, M.] Teledyne Brown Engn Inc, Huntsville, AL 35807 USA.
[Paterson, W.] NASA Headquarders, Washington, DC USA.
[Saito, Y.] YS Design, Tokyo, Japan.
[Schuster, D.] Vantage Syst Inc, Lanham, MD USA.
[Sher, D.] Design Amer Inc, College Pk, MD USA.
[Tucker, C.] Global Sci & Technol Inc, Greenbelt, MD USA.
[Tull, K.] Jackson & Tull, Greenbelt, MD USA.
RP Pollock, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM craig@denaliscientific.org
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
NR 27
TC 66
Z9 66
U1 4
U2 11
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2016
VL 199
IS 1-4
BP 331
EP 406
DI 10.1007/s11214-016-0245-4
PG 76
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6DI
UT WOS:000374299800013
ER
PT J
AU Young, DT
Burch, JL
Gomez, RG
De Los Santos, A
Miller, GP
Wilson, P
Paschalidis, N
Fuselier, SA
Pickens, K
Hertzberg, E
Pollock, CJ
Scherrer, J
Wood, PB
Donald, ET
Aaron, D
Furman, J
George, D
Gurnee, RS
Hourani, RS
Jacques, A
Johnson, T
Orr, T
Pan, KS
Persyn, S
Pope, S
Roberts, J
Stokes, MR
Trattner, KJ
Webster, JM
AF Young, D. T.
Burch, J. L.
Gomez, R. G.
De Los Santos, A.
Miller, G. P.
Wilson, P.
Paschalidis, N.
Fuselier, S. A.
Pickens, K.
Hertzberg, E.
Pollock, C. J.
Scherrer, J.
Wood, P. B.
Donald, E. T.
Aaron, D.
Furman, J.
George, D.
Gurnee, R. S.
Hourani, R. S.
Jacques, A.
Johnson, T.
Orr, T.
Pan, K. S.
Persyn, S.
Pope, S.
Roberts, J.
Stokes, M. R.
Trattner, K. J.
Webster, J. M.
TI Hot Plasma Composition Analyzer for the Magnetospheric Multiscale
Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Plasma ion composition; Reconnection measurements; Time-of-Flight mass
spectrometry
ID ION COMPOSITION; MASS-SPECTROMETER; RECONNECTION; DYNAMICS
AB This paper describes the science motivation, measurement objectives, performance requirements, detailed design, approach and implementation, and calibration of the four Hot Plasma Composition Analyzers (HPCA) for the Magnetospheric Multiscale mission. The HPCA is based entirely on electrostatic optics combining an electrostatic energy analyzer with a carbon-foil based time-of-flight analyzer. In order to fulfill mission requirements, the HPCA incorporates three unique technologies that give it very wide dynamic range capabilities essential to measuring minor ion species in the presence of extremely high proton fluxes found in the region of magnetopause reconnection. Dynamic range is controlled primarily by a novel radio frequency system analogous to an RF mass spectrometer. The RF, in combination with capabilities for high TOF event processing rates and high current micro-channel plates, ensures the dynamic range and sensitivity needed for accurate measurements of ion fluxes between similar to 1 eV and 40 keV that are expected in the region of reconnection events. A third technology enhances mass resolution in the presence of high proton flux.
In order to calibrate the four HPCA instruments we have developed a unique ion calibration system. The system delivers a multi-species beam resolved to M/Delta M similar to 100 and current densities between 0.05 and 200 pA/cm(2) with a stability of +/- 5 %. The entire system is controlled by a dedicated computer synchronized with the HPCA ground support equipment. This approach results not only in accurate calibration but also in a comprehensive set of coordinated instrument and auxiliary data that makes analysis straightforward and ensures archival of all relevant data.
C1 [Young, D. T.; Burch, J. L.; Gomez, R. G.; De Los Santos, A.; Miller, G. P.; Wilson, P.; Fuselier, S. A.; Pickens, K.; Scherrer, J.; Wood, P. B.; Aaron, D.; Furman, J.; George, D.; Johnson, T.; Orr, T.; Pan, K. S.; Persyn, S.; Pope, S.; Roberts, J.; Webster, J. M.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA.
[Hertzberg, E.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA.
[Donald, E. T.; Gurnee, R. S.; Hourani, R. S.; Stokes, M. R.] Johns Hopkins Univ, Appl Phys Lab, Space Explorat Sect, Johns Hopkins Rd, Laurel, MD 20723 USA.
[Paschalidis, N.; Jacques, A.] NASA, Goddard Space Flight Ctr, Code 670, Greenbelt, MD 20771 USA.
[Pollock, C. J.] NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA.
[Trattner, K. J.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
RP Young, DT (reprint author), SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA.
EM dyoung@swri.edu
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU SwRI Internal Research program; NASA MMS [NNG04EB99C]; SwRI [599789Q,
899039BT]
FX Development of the HPCA has been an ongoing effort at SwRI for the past
10 years. We acknowledge generous support by the SwRI Internal Research
program. We wish to thank members of the staff at SwRI, in particular
W.C. Gibson and R.K. Black for their management skills directing the
SwRI portions of the mission. We thank APL staff members and the APL
internal research program for supporting development of the TOF ASICs
and TOF board. At LMATC we particularly wish to thank Alex Price. We
also acknowledge the support of members of the MMS project staff who
helped with accommodating HPCA on the MMS spacecraft. HPCA was developed
under NASA MMS contract NNG04EB99C. Work at APL was performed under SwRI
subcontract 599789Q and at Lockheed Martin under SwRI subcontract
899039BT.
NR 28
TC 11
Z9 11
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2016
VL 199
IS 1-4
BP 407
EP 470
DI 10.1007/s11214-014-0119-6
PG 64
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6DI
UT WOS:000374299800014
ER
PT J
AU Mauk, BH
Blake, JB
Baker, DN
Clemmons, JH
Reeves, GD
Spence, HE
Jaskulek, SE
Schlemm, CE
Brown, LE
Cooper, SA
Craft, JV
Fennell, JF
Gurnee, RS
Hammock, CM
Hayes, JR
Hill, PA
Ho, GC
Hutcheson, JC
Jacques, AD
Kerem, S
Mitchell, DG
Nelson, KS
Paschalidis, NP
Rossano, E
Stokes, MR
Westlake, JH
AF Mauk, B. H.
Blake, J. B.
Baker, D. N.
Clemmons, J. H.
Reeves, G. D.
Spence, H. E.
Jaskulek, S. E.
Schlemm, C. E.
Brown, L. E.
Cooper, S. A.
Craft, J. V.
Fennell, J. F.
Gurnee, R. S.
Hammock, C. M.
Hayes, J. R.
Hill, P. A.
Ho, G. C.
Hutcheson, J. C.
Jacques, A. D.
Kerem, S.
Mitchell, D. G.
Nelson, K. S.
Paschalidis, N. P.
Rossano, E.
Stokes, M. R.
Westlake, J. H.
TI The Energetic Particle Detector (EPD) Investigation and the Energetic
Ion Spectrometer (EIS) for the Magnetospheric Multiscale (MMS) Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE NASA mission; Magnetospheric multiscale; Magnetosphere; Magnetic
reconnection; Space plasma; Particle acceleration
ID PLASMA SHEET ION; MAGNETIC RECONNECTION; MAGNETOTAIL RECONNECTION;
ELECTRON ACCELERATION; FIELD; DISTRIBUTIONS; ENERGIZATION; INSTRUMENT;
SPACECRAFT; MECHANISM
AB The Energetic Particle Detector (EPD) Investigation is one of 5 fields-and-particles investigations on the Magnetospheric Multiscale (MMS) mission. MMS comprises 4 spacecraft flying in close formation in highly elliptical, near-Earth-equatorial orbits targeting understanding of the fundamental physics of the important physical process called magnetic reconnection using Earth's magnetosphere as a plasma laboratory. EPD comprises two sensor types, the Energetic Ion Spectrometer (EIS) with one instrument on each of the 4 spacecraft, and the Fly's Eye Energetic Particle Spectrometer (FEEPS) with 2 instruments on each of the 4 spacecraft. EIS measures energetic ion energy, angle and elemental compositional distributions from a required low energy limit of 20 keV for protons and 45 keV for oxygen ions, up to > 0.5 MeV (with capabilities to measure up to > 1 MeV). FEEPS measures instantaneous all sky images of energetic electrons from 25 keV to > 0.5 MeV, and also measures total ion energy distributions from 45 keV to > 0.5 MeV to be used in conjunction with EIS to measure all sky ion distributions. In this report we describe the EPD investigation and the details of the EIS sensor. Specifically we describe EPD-level science objectives, the science and measurement requirements, and the challenges that the EPD team had in meeting these requirements. Here we also describe the design and operation of the EIS instruments, their calibrated performances, and the EIS in-flight and ground operations. Blake et al. (The Flys Eye Energetic Particle Spectrometer (FEEPS) contribution to the Energetic Particle Detector (EPD) investigation of the Magnetospheric Magnetoscale (MMS) Mission, this issue) describe the design and operation of the FEEPS instruments, their calibrated performances, and the FEEPS in-flight and ground operations. The MMS spacecraft will launch in early 2015, and over its 2-year mission will provide comprehensive measurements of magnetic reconnection at Earth's magnetopause during the 18 months that comprise orbital phase 1, and magnetic reconnection within Earth's magnetotail during the about 6 months that comprise orbital phase 2.
C1 [Mauk, B. H.; Jaskulek, S. E.; Schlemm, C. E.; Brown, L. E.; Cooper, S. A.; Gurnee, R. S.; Hayes, J. R.; Hill, P. A.; Ho, G. C.; Hutcheson, J. C.; Kerem, S.; Mitchell, D. G.; Nelson, K. S.; Stokes, M. R.; Westlake, J. H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Blake, J. B.; Clemmons, J. H.; Fennell, J. F.] Aerosp Corp, El Segundo, CA 90245 USA.
[Baker, D. N.; Craft, J. V.] Univ Colorado, LASP, Boulder, CO 80309 USA.
[Spence, H. E.] Univ New Hampshire, Durham, NH 03824 USA.
[Reeves, G. D.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Jacques, A. D.; Paschalidis, N. P.; Rossano, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Hammock, C. M.] NASA, Johnson Space Ctr, Houston, TX USA.
RP Mauk, BH (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
EM barry.mauk@jhuapl.edu
RI NASA MMS, Science Team/J-5393-2013; Mauk, Barry/E-8420-2017;
OI NASA MMS, Science Team/0000-0002-9504-5214; Mauk,
Barry/0000-0001-9789-3797; Clemmons, James/0000-0002-5298-5222; Reeves,
Geoffrey/0000-0002-7985-8098
NR 46
TC 23
Z9 23
U1 0
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2016
VL 199
IS 1-4
BP 471
EP 514
DI 10.1007/s11214-014-0055-5
PG 44
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6DI
UT WOS:000374299800015
ER
PT J
AU Baker, DN
Riesberg, L
Pankratz, CK
Panneton, RS
Giles, BL
Wilder, FD
Ergun, RE
AF Baker, D. N.
Riesberg, L.
Pankratz, C. K.
Panneton, R. S.
Giles, B. L.
Wilder, F. D.
Ergun, R. E.
TI Magnetospheric Multiscale Instrument Suite Operations and Data System
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Data Management; Acquisition; Science Operations; Instrument Operations;
Data Products; Data Access; Data Center
AB The four Magnetospheric Multiscale (MMS) spacecraft will collect a combined volume of similar to 100 gigabits per day of particle and field data. On average, only 4 gigabits of that volume can be transmitted to the ground. To maximize the scientific value of each transmitted data segment, MMS has developed the Science Operations Center (SOC) to manage science operations, instrument operations, and selection, downlink, distribution, and archiving of MMS science data sets. The SOC is managed by the Laboratory for Atmospheric and Space Physics (LASP) in Boulder, Colorado and serves as the primary point of contact for community participation in the mission. MMS instrument teams conduct their operations through the SOC, and utilize the SOC's Science Data Center (SDC) for data management and distribution. The SOC provides a single mission data archive for the housekeeping and science data, calibration data, ephemerides, attitude and other ancillary data needed to support the scientific use and interpretation. All levels of data products will reside at and be publicly disseminated from the SDC. Documentation and metadata describing data products, algorithms, instrument calibrations, validation, and data quality will be provided. Arguably, the most important innovation developed by the SOC is the MMS burst data management and selection system. With nested automation and "Scientist-in-the-Loop" (SITL) processes, these systems are designed to maximize the value of the burst data by prioritizing the data segments selected for transmission to the ground. This paper describes the MMS science operations approach, processes and data systems, including the burst system and the SITL concept.
C1 [Baker, D. N.; Riesberg, L.; Pankratz, C. K.; Panneton, R. S.; Wilder, F. D.; Ergun, R. E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Giles, B. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Baker, DN (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
EM daniel.baker@lasp.colorado.edu
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU SwRI under NASA program [599791Q, NNG04BB99C, 1541955]
FX The authors thank Southwest Research Institute (SwRI) leadership and the
many science investigators on the Magnetospheric Multiscale mission for
their cooperation. Thanks also go to management and operations
colleagues at NASA Goddard Space Flight Center (GSFC). We especially
acknowledge the efforts of mission operations and data systems personnel
at the Laboratory for Atmospheric and Space Physics. This work was
supported by SwRI subcontract 599791Q under NASA program NNG04BB99C
(Project# 1541955).
NR 4
TC 2
Z9 2
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2016
VL 199
IS 1-4
BP 545
EP 575
DI 10.1007/s11214-014-0128-5
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6DI
UT WOS:000374299800017
ER
PT J
AU Hesse, M
Aunai, N
Birn, J
Cassak, P
Denton, RE
Drake, JF
Gombosi, T
Hoshino, M
Matthaeus, W
Sibeck, D
Zenitani, S
AF Hesse, M.
Aunai, N.
Birn, J.
Cassak, P.
Denton, R. E.
Drake, J. F.
Gombosi, T.
Hoshino, M.
Matthaeus, W.
Sibeck, D.
Zenitani, S.
TI Theory and Modeling for the Magnetospheric Multiscale Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Magnetic reconnection; Magnetospheric multiscale; Particle acceleration;
Dissipation; Turbulence; Plasma theory
ID COLLISIONLESS MAGNETIC RECONNECTION; SOLAR-WIND; ELECTRON ACCELERATION;
DAYSIDE MAGNETOPAUSE; KINETIC SIMULATIONS; FIELD MEASUREMENTS; MHD
SIMULATIONS; GUIDE-FIELD; EVENTS; PLASMA
AB The Magnetospheric Multiscale (MMS) mission will provide measurement capabilities, which will exceed those of earlier and even contemporary missions by orders of magnitude. MMS will, for the first time, be able to measure directly and with sufficient resolution key features of the magnetic reconnection process, down to the critical electron scales, which need to be resolved to understand how reconnection works. Owing to the complexity and extremely high spatial resolution required, no prior measurements exist, which could be employed to guide the definition of measurement requirements, and consequently set essential parameters for mission planning and execution. Insight into expected details of the reconnection process could hence only been obtained from theory and modern kinetic modeling. This situation was recognized early on by MMS leadership, which supported the formation of a fully integrated Theory and Modeling Team (TMT). The TMT participated in all aspects of mission planning, from the proposal stage to individual aspects of instrument performance characteristics. It provided and continues to provide to the mission the latest insights regarding the kinetic physics of magnetic reconnection, as well as associated particle acceleration and turbulence, assuring that, to the best of modern knowledge, the mission is prepared to resolve the inner workings of the magnetic reconnection process. The present paper provides a summary of key recent results or reconnection research by TMT members.
C1 [Hesse, M.; Sibeck, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Aunai, N.] Inst Res Astrophys & Planetol, Toulouse, France.
[Birn, J.] Space Sci Inst, Boulder, CO USA.
[Cassak, P.] W Virginia Univ, Morgantown, WV 26506 USA.
[Denton, R. E.] Dartmouth Coll, Hanover, NH 03755 USA.
[Drake, J. F.] Univ Maryland, College Pk, MD 20742 USA.
[Gombosi, T.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Hoshino, M.] Univ Tokyo, Tokyo, Japan.
[Matthaeus, W.] Univ Delaware, Newark, DE USA.
[Zenitani, S.] Natl Astron Observ Japan, Tokyo, Japan.
RP Hesse, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM michael.hesse@nasa.gov
RI NASA MMS, Science Team/J-5393-2013; Zenitani, Seiji/D-7988-2013;
Gombosi, Tamas/G-4238-2011
OI NASA MMS, Science Team/0000-0002-9504-5214; Zenitani,
Seiji/0000-0002-0945-1815; Gombosi, Tamas/0000-0001-9360-4951
NR 292
TC 9
Z9 9
U1 3
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2016
VL 199
IS 1-4
BP 577
EP 630
DI 10.1007/s11214-014-0078-y
PG 54
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6DI
UT WOS:000374299800018
ER
PT J
AU Goldstein, ML
Ashour-Abdalla, M
Vinas, AF
Dorelli, J
Wendel, D
Klimas, A
Hwang, KJ
El-Alaoui, M
Walker, RJ
Pan, QJ
Liang, HM
AF Goldstein, Melvyn L.
Ashour-Abdalla, Maha
Vinas, Adolfo F.
Dorelli, John
Wendel, Deirdre
Klimas, Alex
Hwang, Kyoung-Joo
El-Alaoui, Mostafa
Walker, Raymond J.
Pan, Qingjiang
Liang, Haoming
TI Mission Oriented Support and Theory (MOST) for MMS-the Goddard Space
Flight Center/University of California Los Angeles Interdisciplinary
Science Program
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Magnetic reconnection; Plasma physics; Magnetofluid turbulence
ID PARALLEL ELECTRIC-FIELDS; TURBULENT MAGNETIC RECONNECTION;
SELF-ORGANIZED CRITICALITY; MAGNETOTAIL CURRENT SHEET; EARTHS PLASMA
SHEET; LOCALIZED RECONNECTION; KINEMATIC RECONNECTION; CLUSTER
OBSERVATIONS; CHARGED-PARTICLES; ALIGNED CURRENT
AB The MOST IDS team was tasked with focusing on two general areas: The first was to participate with the Fast Plasma Investigation (FPI) team in the development of virtual detectors that model the instrument responses of the MMS FPI sensors. The virtual instruments can be "flown through" both simulation data (from magnetohydrodynamic, hybrid, and kinetic simulations) and Cluster and THEMIS spacecraft data. The goal is to determine signatures of magnetic reconnection expected during the MMS mission. Such signatures can serve as triggers for selection of burst mode downloads. The chapter contributed by the FPI team covers that effort in detail and, therefore, most of that work has not been included here. The second area of emphasis, and the one detailed in this chapter, was to build on past and present knowledge of magnetic reconnection and its physical signatures. Below we describe intensive analyses of Cluster and THEMIS data together with theoretical models and simulations that delineate the plasma signatures that surround sites of reconnection, including the effects of turbulence as well as the detailed kinetic signatures that indicate proximity to reconnection sites. In particular, we point out that particles are energized in several regions, not only at the actual site of reconnection.
C1 [Goldstein, Melvyn L.; Ashour-Abdalla, Maha; Vinas, Adolfo F.; Dorelli, John; Wendel, Deirdre; Klimas, Alex; Hwang, Kyoung-Joo] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Ashour-Abdalla, Maha; El-Alaoui, Mostafa] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[El-Alaoui, Mostafa; Pan, Qingjiang; Liang, Haoming] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA.
[Walker, Raymond J.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA.
[Klimas, Alex; Hwang, Kyoung-Joo] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
RP Goldstein, ML (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM melvyn.l.goldstein@nasa.gov
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
NR 132
TC 2
Z9 2
U1 2
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2016
VL 199
IS 1-4
BP 689
EP 719
DI 10.1007/s11214-014-0127-6
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6DI
UT WOS:000374299800021
ER
PT J
AU Reiff, PH
Cline, TD
AF Reiff, Patricia H.
Cline, Troy D.
TI Education and Communication for the Magnetospheric Multiscale Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Magnetism; Education; Communication; Outreach; E/PO; Informal education;
Heliosphere; Magnetic fields; Software; Vodcast; Podcast; iBooks;
Planetarium; Social media; Underserved students; Teachers; CoSTEM; Next
generation science standards; Evaluation; Metrics
AB The Magnetospheric Multiscale mission (MMS) proposed a balanced portfolio of education and communication activities and products, including broadly distributed materials for the general public, special programs and materials for teachers, targeted activities and materials for underserved groups, and intensive experiences for future scientists and engineers. Our plan includes creation and dissemination of educational software, podcasts and vodcasts, planetarium shows, teacher and student activities, 3D models, social media and smartphone apps. We have surveyed users of NASA data to determine which modes of learning were effective in their youth and which are the most effective now, and use those results to inform our education and communication plans. All materials will be reviewed and placed in NASA online educational archives for broad dissemination.
C1 [Reiff, Patricia H.] Rice Univ, Houston, TX USA.
[Cline, Troy D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Reiff, PH (reprint author), Rice Univ, Houston, TX USA.
EM reiff@rice.edu
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
NR 12
TC 0
Z9 0
U1 1
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAR
PY 2016
VL 199
IS 1-4
BP 721
EP 747
DI 10.1007/s11214-015-0166-7
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DJ6DI
UT WOS:000374299800022
ER
PT J
AU Case, NA
MacDonald, EA
Viereck, R
AF Case, N. A.
MacDonald, E. A.
Viereck, R.
TI Using citizen science reports to define the equatorial extent of auroral
visibility
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE aurora; visibility; citizen science
ID STATISTICAL-MODEL; ENERGY FLUX; PRECIPITATION
AB An aurora may often be viewed hundreds of kilometers equatorward of the auroral oval owing to its altitude. As such, the NOAA Space Weather Prediction Center (SWPC) Aurora Forecast product provides a view line to demonstrate the equatorial extent of auroral visibility, assuming that it is sufficiently bright and high in altitude. The view line in the SWPC product is based upon the latitude of the brightest aurora, for each hemisphere, as specified by the real-time oval variation, assessment, tracking, intensity, and online nowcasting (OVATION) Prime (2010) aurora precipitation model. In this study, we utilize nearly 500 citizen science auroral reports to compare with the view line provided by an updated SWPC aurora forecast product using auroral precipitation data from OVATION Prime (2013). The citizen science observations were recorded during March and April 2015 using the Aurorasaurus platform and cover one large geomagnetic storm and several smaller events. We find that this updated SWPC view line is conservative in its estimate and that the aurora is often viewable further equatorward than is indicated by the forecast. By using the citizen reports to modify the scaling parameters used to link the OVATION Prime (2013) model to the view line, we produce a new view line estimate that more accurately represents the equatorial extent of visible aurora. An OVATION Prime (2013) energy flux-based equatorial boundary view line is also developed and is found to provide the best overall agreement with the citizen science reports, with an accuracy of 91%.
C1 [Case, N. A.; MacDonald, E. A.] New Mexico Consortium, Los Alamos, NM USA.
[Case, N. A.; MacDonald, E. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Case, N. A.] Univ Lancaster, Dept Phys, Lancaster, England.
[Viereck, R.] NOAA, Space Weather Predict Ctr, Boulder, CO USA.
RP Case, NA (reprint author), New Mexico Consortium, Los Alamos, NM USA.; Case, NA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.; Case, NA (reprint author), Univ Lancaster, Dept Phys, Lancaster, England.
EM n.case@lancaster.ac.uk
OI Case, Nathan/0000-0003-0692-1778
FU National Science Foundation (NSF) [1344296]
FX This material is based upon work supported, in part, by the National
Science Foundation (NSF) under grant 1344296. Any opinions, findings,
and conclusions or recommendations expressed in this material are those
of the author(s) and do not necessarily reflect the views of NSF. The
OVATION Prime output and associated view line were kindly supplied by
the Space Weather Prediction Center, Boulder, CO, National Oceanic and
Atmospheric Administration (NOAA), U.S. Department of Commerce. The
output can be freely downloaded from the NOAA SWPC product pages
(http://www.swpc.noaa.gov/products/aurora-30-minute-forecast).
NR 22
TC 1
Z9 1
U1 2
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD MAR
PY 2016
VL 14
IS 3
BP 198
EP 209
DI 10.1002/2015SW001320
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA DK1UB
UT WOS:000374698800002
ER
PT J
AU Adriani, O
Barbarino, GC
Bazilevskaya, GA
Bellotti, R
Boezio, M
Bogomolov, EA
Bongi, M
Bonvicini, V
Bottai, S
Bruno, A
Cafagna, F
Campana, D
Carlson, P
Casolino, M
Castellini, G
De Donato, C
de Nolfo, GA
De Santis, C
De Simone, N
Di Felice, V
Galper, AM
Karelin, AV
Koldashov, SV
Koldobskiy, S
Krutkov, SY
Kvashnin, AN
Leonov, A
Malakhov, V
Marcelli, L
Martucci, M
Mayorov, AG
Menn, W
Merge, M
Mikhailov, VV
Mocchiutti, E
Monaco, A
Mori, N
Munini, R
Osteria, G
Palma, F
Panico, B
Papini, P
Pearce, M
Picozza, P
Ricci, M
Ricciarini, SB
Sarkar, R
Scotti, V
Simon, M
Sparvoli, R
Spillantini, P
Stozhkov, YI
Vacchi, A
Vannuccini, E
Vasilyev, GI
Voronov, SA
Yurkin, YT
Zampa, G
Zampa, N
AF Adriani, O.
Barbarino, G. C.
Bazilevskaya, G. A.
Bellotti, R.
Boezio, M.
Bogomolov, E. A.
Bongi, M.
Bonvicini, V.
Bottai, S.
Bruno, A.
Cafagna, F.
Campana, D.
Carlson, P.
Casolino, M.
Castellini, G.
De Donato, C.
de Nolfo, G. A.
De Santis, C.
De Simone, N.
Di Felice, V.
Galper, A. M.
Karelin, A. V.
Koldashov, S. V.
Koldobskiy, S.
Krutkov, S. Y.
Kvashnin, A. N.
Leonov, A.
Malakhov, V.
Marcelli, L.
Martucci, M.
Mayorov, A. G.
Menn, W.
Merge, M.
Mikhailov, V. V.
Mocchiutti, E.
Monaco, A.
Mori, N.
Munini, R.
Osteria, G.
Palma, F.
Panico, B.
Papini, P.
Pearce, M.
Picozza, P.
Ricci, M.
Ricciarini, S. B.
Sarkar, R.
Scotti, V.
Simon, M.
Sparvoli, R.
Spillantini, P.
Stozhkov, Y. I.
Vacchi, A.
Vannuccini, E.
Vasilyev, G. I.
Voronov, S. A.
Yurkin, Y. T.
Zampa, G.
Zampa, N.
TI PAMELA's measurements of geomagnetic cutoff variations during the 14
December 2006 storm
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE Geomagnetic Cutoff; Magnetic Storms; Solar Energetic Particles
ID COSMIC-RAY PHYSICS; COORDINATE SYSTEM; MAGNETIC-FIELD; SOLAR-WIND;
MAGNETOSPHERE; MODEL; RIGIDITIES; LATITUDES
AB Data from the Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA) satellite experiment were used to measure the geomagnetic cutoff for high-energy ( 80MeV) protons during the 14 December 2006 geomagnetic storm. The variations of the cutoff latitude as a function of rigidity were studied on relatively short timescales, corresponding to spacecraft orbital periods (approximate to 94 min). Estimated cutoff values were compared with those obtained by means of a trajectory-tracing approach based on a dynamical empirical modeling of the Earth's magnetosphere. We found significant variations in the cutoff latitude, with a maximum suppression of approximate to 7 degrees at lowest rigidities during the main phase of the storm. The observed reduction in the geomagnetic shielding and its temporal evolution were related to the changes in the magnetospheric configuration, investigating the role of interplanetary magnetic field, solar wind, and geomagnetic parameters. PAMELA's results represent the first direct measurement of geomagnetic cutoffs for protons with kinetic energies in the sub-GeV and GeV region.
C1 [Adriani, O.; Bongi, M.; Mori, N.] Univ Florence, Dept Phys & Astron, Sesto Fiorentino, Italy.
[Adriani, O.; Bongi, M.; Bottai, S.; Mori, N.; Papini, P.; Ricciarini, S. B.; Vannuccini, E.] Ist Nazl Fis Nucl, Sez Florence, Sesto Fiorentino, Italy.
[Barbarino, G. C.; Scotti, V.] Univ Naples Federico II, Dept Phys, Naples, Italy.
[Barbarino, G. C.; Campana, D.; Osteria, G.; Panico, B.; Scotti, V.] Ist Nazl Fis Nucl, Sez Naples, I-80125 Naples, Italy.
[Bazilevskaya, G. A.; Kvashnin, A. N.; Stozhkov, Y. I.] PN Lebedev Phys Inst, Leninsky Prospect 53, Moscow 117924, Russia.
[Bellotti, R.; Bruno, A.; Monaco, A.] Univ Bari, Dept Phys, Bari, Italy.
[Bellotti, R.; Bruno, A.; Cafagna, F.; Monaco, A.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Boezio, M.; Bonvicini, V.; Mocchiutti, E.; Munini, R.; Vacchi, A.; Zampa, G.; Zampa, N.] Ist Nazl Fis Nucl, Sez Trieste, Trieste, Italy.
[Bogomolov, E. A.; Krutkov, S. Y.; Vasilyev, G. I.] AF Ioffe Phys Tech Inst, Politekhnicheskaya 26, St Petersburg 194021, Russia.
[Carlson, P.; Pearce, M.] KTH, Dept Phys, Stockholm, Sweden.
[Carlson, P.; Pearce, M.] AlbaNova Univ Ctr, Oskar Klein Ctr Cosmoparticle Phys, Stockholm, Sweden.
[Casolino, M.; De Donato, C.; De Santis, C.; De Simone, N.; Di Felice, V.; Marcelli, L.; Merge, M.; Osteria, G.; Sparvoli, R.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, Rome, Italy.
[Casolino, M.] RIKEN, Adv Sci Inst, Wako, Saitama, Japan.
[Castellini, G.; Ricciarini, S. B.] IFAC, Sesto Fiorentino, Italy.
[De Donato, C.; De Santis, C.; Marcelli, L.; Martucci, M.; Merge, M.; Osteria, G.; Picozza, P.; Sparvoli, R.] Univ Roma Tor Vergata, Dept Phys, Rome, Italy.
[de Nolfo, G. A.] NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD USA.
[Di Felice, V.] Agenzia Spaziale Italiana Sci Data Ctr, Rome, Italy.
[Galper, A. M.; Karelin, A. V.; Koldashov, S. V.; Koldobskiy, S.; Leonov, A.; Malakhov, V.; Mayorov, A. G.; Mikhailov, V. V.; Voronov, S. A.; Yurkin, Y. T.] Natl Res Nucl Univ MEPhI, Moscow, Russia.
[Martucci, M.; Ricci, M.] Ist Nazl Fis Nucl, Lab Nazl Frascati, POB 13, I-00044 Frascati, Italy.
[Menn, W.; Simon, M.] Univ Siegen, Dept Phys, D-57068 Siegen, Germany.
[Munini, R.] Univ Trieste, Dept Phys, Trieste, Italy.
[Sarkar, R.] Indian Ctr Space Phys, Kolkata, W Bengal, India.
[Sarkar, R.] Ist Nazl Fis Nucl, Sez Trieste, Trieste, Italy.
[Spillantini, P.] IAPS INAF, I-00133 Rome, Italy.
RP Bruno, A (reprint author), Univ Bari, Dept Phys, Bari, Italy.; Bruno, A (reprint author), Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
EM Alessandro.Bruno@ba.infn.it
RI Mayorov, Andrey/M-1207-2016; Mikhailov, Vladimir/B-5368-2014; Krutkov,
Sergey/E-7561-2014; Koldobskiy, Sergey/K-6507-2015; Leonov,
Alexey/E-4698-2016; Vasilyev, Gennady/E-4843-2014; De Donato,
Cinzia/J-9132-2015; De Santis, Cristian/C-1210-2011; Cafagna,
Francesco/A-9299-2010; marcelli, laura/K-8860-2016; Palma,
Francesco/K-3224-2015; Di Felice, Valeria/L-2989-2016; Mori,
Nicola/D-9459-2016; Karelin, Alexander/O-6576-2016; Voronov,
Sergey/P-9654-2016; Malakhov, Vitaly/Q-6730-2016; Bazilevskaya,
Galina/M-6175-2015; Panico, Beatrice/F-1137-2017; Vacchi,
Andrea/C-1291-2010;
OI Mikhailov, Vladimir/0000-0003-3851-2901; Koldobskiy,
Sergey/0000-0001-9187-0383; De Donato, Cinzia/0000-0002-9725-1281; De
Santis, Cristian/0000-0002-7280-2446; Cafagna,
Francesco/0000-0002-7450-4784; marcelli, laura/0000-0002-3180-1228;
Palma, Francesco/0000-0001-7076-8830; Mori, Nicola/0000-0003-2138-3787;
Voronov, Sergey/0000-0002-9209-0618; Panico,
Beatrice/0000-0003-1063-6961; Ricciarini, Sergio
Bruno/0000-0001-6176-3368; Vacchi, Andrea/0000-0003-3855-5856; Boezio,
Mirko/0000-0002-8015-2981
FU Italian Space Agency (ASI); Deutsches Zentrum fur Luftund Raumfahrt
(DLR); Swedish National Space Board; Swedish Research Council; Russian
Space Agency (Roscosmos); Russian Scientific Foundation
FX We acknowledge support from The Italian Space Agency (ASI), Deutsches
Zentrum fur Luftund Raumfahrt (DLR), The Swedish National Space Board,
The Swedish Research Council, The Russian Space Agency (Roscosmos), and
The Russian Scientific Foundation.
NR 45
TC 2
Z9 2
U1 9
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD MAR
PY 2016
VL 14
IS 3
BP 210
EP 220
DI 10.1002/2016SW001364
PG 11
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA DK1UB
UT WOS:000374698800003
ER
PT J
AU Glotter, MJ
Moyer, EJ
Ruane, AC
Elliott, JW
AF Glotter, Michael J.
Moyer, Elisabeth J.
Ruane, Alex C.
Elliott, Joshua W.
TI Evaluating the Sensitivity of Agricultural Model Performance to
Different Climate Inputs
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID DAILY PRECIPITATION; UNITED-STATES; CROP YIELDS; TEMPERATURE; SYSTEM;
PROTOCOLS; DATASETS; IMPACT; US
AB Projections of future food production necessarily rely on models, which must themselves be validated through historical assessments comparing modeled and observed yields. Reliable historical validation requires both accurate agricultural models and accurate climate inputs. Problems with either may compromise the validation exercise. Previous studies have compared the effects of different climate inputs on agricultural projections but either incompletely or without a ground truth of observed yields that would allow distinguishing errors due to climate inputs from those intrinsic to the crop model. This study is a systematic evaluation of the reliability of a widely used crop model for simulating U.S. maize yields when driven by multiple observational data products. The parallelized Decision Support System for Agrotechnology Transfer (pDSSAT) is driven with climate inputs from multiple sources-reanalysis, reanalysis that is bias corrected with observed climate, and a control dataset and compared with observed historical yields. The simulations show that model output is more accurate when driven by any observation-based precipitation product than when driven by non-bias-corrected reanalysis. The simulations also suggest, in contrast to previous studies, that biased precipitation distribution is significant for yields only in arid regions. Some issues persist for all choices of climate inputs: crop yields appear to be oversensitive to precipitation fluctuations but under sensitive to floods and heat waves. These results suggest that the most important issue for agricultural projections may be not climate inputs but structural limitations in the crop models themselves.
C1 [Glotter, Michael J.; Moyer, Elisabeth J.] Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA.
[Ruane, Alex C.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Elliott, Joshua W.] Univ Chicago, Computat Inst, Chicago, IL 60637 USA.
RP Glotter, MJ (reprint author), Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA.
EM glotter@uchicago.edu
FU NSF through the Decision Making Under Uncertainty program [SES-0951576];
NASA's Indicators for the National Climate Assessment program; NSF
Graduate Fellowship [DGE-1144082]; NSF SEES Fellowship [1215910]; NSF
[OCI-1148443]; AgMIP community
FX This research was performed as part of the Center for Robust
Decision-Making on Climate and Energy Policy (RDCEP) at The University
of Chicago. RDCEP is funded by a grant from NSF (SES-0951576) through
the Decision Making Under Uncertainty program. This work was also funded
in part by a grant from NASA's Indicators for the National Climate
Assessment program. Author MG acknowledges support of an NSF Graduate
Fellowship (DGE-1144082) and JE acknowledges an NSF SEES Fellowship
(1215910). CPC US Unified Precipitation data were downloaded on 3 March
2011 from the NOAA/OAR/ESRL PSD, Boulder, Colorado, from their website
at http://www.esrl.noaa.gov/psd/. SRB solar data were obtained from the
NASA Langley Research Center Atmospheric Sciences Data Center NASA/GEWEX
SRB Project. Computing for this project was facilitated using the Swift
parallel scripting language (NSF Grant OCI-1148443). Computing support
and data storage were provided by the University of Chicago Research
Computing Center. We thank the AgMIP community for support of this
effort.
NR 53
TC 1
Z9 1
U1 6
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD MAR
PY 2016
VL 55
IS 3
BP 579
EP 594
DI 10.1175/JAMC-D-15-0120.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DJ4VN
UT WOS:000374206300005
ER
PT J
AU Kuo, KS
Olson, WS
Johnson, BT
Grecu, M
Tian, L
Clune, TL
van Aartsen, BH
Heymsfield, AJ
Liao, L
Meneghini, R
AF Kuo, Kwo-Sen
Olson, William S.
Johnson, Benjamin T.
Grecu, Mircea
Tian, Lin
Clune, Thomas L.
van Aartsen, Bruce H.
Heymsfield, Andrew J.
Liao, Liang
Meneghini, Robert
TI The Microwave Radiative Properties of Falling Snow Derived from
Nonspherical Ice Particle Models. Part I: An Extensive Database of
Simulated Pristine Crystals and Aggregate Particles, and Their
Scattering Properties
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID RAYLEIGH-GANS APPROXIMATION; DISCRETE-DIPOLE APPROXIMATION;
PRECIPITATING CLOUDS; RADAR BACKSCATTERING; PROFILING ALGORITHM; SIZE
DISTRIBUTIONS; SITU OBSERVATIONS; SNOWFLAKES; FREQUENCIES; HYDROMETEORS
AB A 3D growth model is used to simulate pristine ice crystals, which are aggregated using a collection algorithm to create larger, multicrystal particles. The simulated crystals and aggregates have mass-versus-size and fractal properties that are consistent with field observations. The growth/collection model is used to generate a large database of snow particles, and the single-scattering properties of each particle are computed using the discrete dipole approximation to account for the nonspherical geometries of the particles. At 13.6 and 35.5 GHz, the bulk radar reflectivities of nonspherical snow particle polydispersions differ from those of more approximate spherical, homogeneous, ice-air particle polydispersions that have the same particle size distributions, although the reflectivities of the nonspherical particles are roughly approximated by polydispersions of spheres of 0.1-0.2 g cm(-3) density. At higher microwave frequencies, such as 165.5 GHz, the bulk extinction (and scattering) coefficients of the nonspherical snow polydispersions are comparable to those of low-density spheres, but the asymmetry parameters of the nonspherical particles are substantially less than those of spheres for a broad range of assumed spherical particle densities. Because of differences in the asymmetry of scatter, simulated microwave-scattering depressions using nonspherical particles may well exceed those of spheres for snow layers with the same vertical water path. It may be concluded that, in precipitation remote sensing applications that draw upon input from radar and/or radiometer observations spanning a range of microwave frequencies, nonspherical snow particle models should be used to properly interpret the observations.
C1 [Kuo, Kwo-Sen] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Olson, William S.; Johnson, Benjamin T.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Grecu, Mircea; Tian, Lin; Liao, Liang] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA.
[Clune, Thomas L.; Meneghini, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[van Aartsen, Bruce H.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Heymsfield, Andrew J.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Johnson, Benjamin T.] Atmospher & Environm Res Inc, Lexington, MA USA.
RP Olson, WS (reprint author), NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM bill.olson@nasa.gov
FU NASA PMM program; NASA RST program; NASA [NNX10AI49G, NNX13AG87G,
NNX11AR53G, NNX11AR55G, NNX13AG48G, NNX10AH67G, NNX13AH73G]
FX The authors thank Janko Gravner and David Griffeath for helpful
discussions that led to the development of the simulations of ice
crystal growth in this study. The bulk of this investigation was
supported by the NASA PMM and RST programs. To be specific, NASA Grants
NNX10AI49G, NNX13AG87G, NNX11AR53G, NNX11AR55G, NNX13AG48G, NNX10AH67G,
and NNX13AH73G provided support. Kwo-Sen Kuo also acknowledges the
generous support of Ziad Haddad and Simone Tanelli.
NR 68
TC 7
Z9 7
U1 2
U2 4
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD MAR
PY 2016
VL 55
IS 3
BP 691
EP 708
DI 10.1175/JAMC-D-15-0130.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DJ4VN
UT WOS:000374206300011
ER
PT J
AU Olson, WS
Tian, L
Grecu, M
Kuo, KS
Johnson, BT
Heymsfield, AJ
Bansemer, A
Heymsfield, GM
Wang, JR
Meneghini, R
AF Olson, William S.
Tian, Lin
Grecu, Mircea
Kuo, Kwo-Sen
Johnson, Benjamin T.
Heymsfield, Andrew J.
Bansemer, Aaron
Heymsfield, Gerald M.
Wang, James R.
Meneghini, Robert
TI The Microwave Radiative Properties of Falling Snow Derived from
Nonspherical Ice Particle Models. Part II: Initial Testing Using Radar,
Radiometer and In Situ Observations
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID TRMM PRECIPITATION RADAR; SCATTERING PARAMETERS; PROFILING ALGORITHM;
SIZE DISTRIBUTIONS; CROSS-SECTIONS; MELTING-LAYER; HYDROMETEORS;
APPROXIMATION; FREQUENCIES; CLOUDS
AB In this study, two different particle models describing the structure and electromagnetic properties of snow are developed and evaluated for potential use in satellite combined radar-radiometer precipitation estimation algorithms. In the first model, snow particles are assumed to be homogeneous ice-air spheres with single scattering properties derived from Mie theory. In the second model, snow particles are created by simulating the self-collection of pristine ice crystals into aggregate particles of different sizes, using different numbers and habits of the collected component crystals. Single-scattering properties of the resulting nonspherical snow particles are determined using the discrete dipole approximation. The size-distribution-integrated scattering properties of the spherical and nonspherical snow particles are incorporated into a dual-wavelength radar profiling algorithm that is applied to 14- and 34-GHz observations of stratiform precipitation from the ER-2 aircraftborne High-Altitude Imaging Wind and Rain Airborne Profiler (HIWRAP) radar. The retrieved ice precipitation profiles are then input to a forward radiative transfer calculation in an attempt to simulate coincident radiance observations from the Conical Scanning Millimeter-Wave Imaging Radiometer (CoSMIR). Much greater consistency between the simulated and observed CoSMIR radiances is obtained using estimated profiles that are based upon the nonspherical crystal/aggregate snow particle model. Despite this greater consistency, there remain some discrepancies between the higher moments of the HIWRAP-retrieved precipitation size distributions and in situ distributions derived from microphysics probe observations obtained from Citation aircraft underflights of the ER-2. These discrepancies can only be eliminated if a subset of lower-density crystal/aggregate snow particles is assumed in the radar algorithm and in the interpretation of the in situ data.
C1 [Olson, William S.; Johnson, Benjamin T.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Tian, Lin; Grecu, Mircea] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA.
[Kuo, Kwo-Sen] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Heymsfield, Andrew J.; Bansemer, Aaron] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Heymsfield, Gerald M.; Wang, James R.; Meneghini, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Johnson, Benjamin T.] Atmospher & Environm Res Inc, Lexington, MA USA.
RP Olson, WS (reprint author), NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM bill.olson@nasa.gov
RI Measurement, Global/C-4698-2015
FU NASA PMM program; NASA RST program; NASA [NNX10AI49G, NNX13AG87G,
NNX11AR53G, NNX11AR55G, NNX10AH67G, NNX13AH73G]
FX The authors acknowledge the many people contributing their data and/or
expertise to this study. These include Lihua Li for providing HIWRAP
data and Gail Skofronick-Jackson for providing CoSMIR observations from
the MC3E campaign. Walter Petersen was a strong advocate for MC3E
aircraft flight plans that led to the collection of these excellent
data. In addition, Liang Liao, Stephen J. Munchak, and David Bolvin made
contributions through very helpful discussions or production of relevant
datasets. The bulk of this investigation was supported by the NASA PMM
and RST programs. To be specific, NASA Grants NNX10AI49G, NNX13AG87G,
NNX11AR53G, NNX11AR55G, NNX10AH67G, and NNX13AH73G provided support.
Kwo-Sen Kuo also acknowledges the generous support of Ziad Haddad and
Simone Tanelli.
NR 50
TC 4
Z9 4
U1 3
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD MAR
PY 2016
VL 55
IS 3
BP 709
EP 722
DI 10.1175/JAMC-D-15-0131.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DJ4VN
UT WOS:000374206300012
ER
PT J
AU Kim, JH
Chan, WN
Sridhar, B
Sharman, RD
Williams, PD
Strahan, M
AF Kim, Jung-Hoon
Chan, William N.
Sridhar, Banavar
Sharman, Robert D.
Williams, Paul D.
Strahan, Matt
TI Impact of the North Atlantic Oscillation on Transatlantic Flight Routes
and Clear-Air Turbulence
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID UPPER-LEVEL TURBULENCE; AVIATION TURBULENCE; CLIMATE-CHANGE; SYSTEM;
CIRRUS; WINTER
AB The variation of wind-optimal transatlantic flight routes and their turbulence potential is investigated to understand how upper-level winds and large-scale flow patterns can affect the efficiency and safety of long-haul flights. In this study, the wind-optimal routes (WORs) that minimize the total flight time by considering wind variations are modeled for flights between John F. Kennedy International Airport (JFK) in New York, New York, and Heathrow Airport (LHR) in London, United Kingdom, during two distinct winter periods of abnormally high and low phases of North Atlantic Oscillation (NAO) teleconnection patterns. Eastbound WORs approximate the JFK LHR great circle (GC) route following northerly shifted jets in the +NAO period. Those WORs deviate southward following southerly shifted jets during the NAO period, because eastbound WORs fly closely to the prevailing westerly jets to maximize tailwinds. Westbound WORs, however, spread meridionally to avoid the jets near the GC in the +NAO period to minimize headwinds. In the NAO period, westbound WORs are north of the GC because of the southerly shifted jets. Consequently, eastbound WORs are faster but have higher probabilities of encountering clear-air turbulence than westbound ones, because eastbound WORs are close to the jet streams, especially near the cyclonic shear side of the jets in the northern (southern) part of the GC in the +NAO ( NAO) period. This study suggests how predicted teleconnection weather patterns can be used for long-haul strategic flight planning, ultimately contributing to minimizing aviation's impact on the environment.
C1 [Kim, Jung-Hoon] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Chan, William N.; Sridhar, Banavar] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Sharman, Robert D.] Natl Ctr Atmospher Res, Res Applicat Lab, POB 3000, Boulder, CO 80307 USA.
[Williams, Paul D.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Kim, Jung-Hoon; Strahan, Matt] NOAA NWS Aviat Weather Ctr, Kansas City, MO USA.
RP Kim, JH (reprint author), 7220 NW 101st Terr, Kansas City, MO 64153 USA.
EM jung-hoon.kim@noaa.gov
RI Williams, Paul/B-2432-2012
OI Williams, Paul/0000-0002-9713-9820
FU U.S. Federal Aviation Administration (FAA)
FX This research is in response to requirements and funding by the U.S.
Federal Aviation Administration (FAA). The views expressed are those of
the authors and do not necessarily represent the official policy and
position of the FAA. The authors thank three anonymous reviewers for
their invaluable comments and suggestions.
NR 31
TC 1
Z9 1
U1 2
U2 4
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD MAR
PY 2016
VL 55
IS 3
BP 763
EP 771
DI 10.1175/JAMC-D-15-0261.1
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DJ4VN
UT WOS:000374206300015
ER
PT J
AU Stuart, JR
Howell, KC
Wilson, RS
AF Stuart, Jeffrey R.
Howell, Kathleen C.
Wilson, Roby S.
TI Design of End-to-End Trojan Asteroid Rendezvous Tours Incorporating
Scientific Value
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID HEKTOR
AB The sun-Jupiter Trojan asteroids are celestial bodies of great scientific interest as well as potential natural assets offering mineral resources for long-term human exploration of the Solar System. Previous investigations have addressed the automated design of tours within the asteroid swarm and the transition of prospective tours to higher-fidelity, end-to-end trajectories. The current development incorporates the route-finding ant colony optimization algorithm into the automated tour-generation procedure. Furthermore, the potential scientific merit of the destination asteroids is incorporated such that encounters with higher-value asteroids are preferentially incorporated during sequence creation.
C1 [Stuart, Jeffrey R.] Purdue Univ, Sch Aeronaut & Astronaut, 701 West Stadium Ave, W Lafayette, IN 47907 USA.
[Howell, Kathleen C.] Purdue Univ, Sch Aeronaut & Astronaut, Aeronaut & Astronaut, 701 West Stadium Ave, W Lafayette, IN 47907 USA.
[Stuart, Jeffrey R.] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Nav & Mission Design Syst Engn Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Wilson, Roby S.] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Inner Planet Mission Anal Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Stuart, JR (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, 701 West Stadium Ave, W Lafayette, IN 47907 USA.; Stuart, JR (reprint author), CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Nav & Mission Design Syst Engn Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU NASA Office of the Chief Technologist's Space Technology Research
Fellowship, NASA [NNX12AM61H]; Purdue Research Foundation
FX This work was conducted at Purdue University and the Jet Propulsion
Laboratory and is supported by a NASA Office of the Chief Technologist's
Space Technology Research Fellowship, NASA grant NNX12AM61H, and the
Purdue Research Foundation. Many thanks to Wayne Schlei, who helped
immensely with the trajectory images and ant colony optimization (ACO)
discussions, and the technical personnel at the Jet Propulsion
Laboratory, Mission Design and Navigation Section. The authors also
acknowledge the contributions of Seokcheon Lee of the Purdue University
School of Industrial Engineering for introducing ACO to the authors.
Andrew Rivkin, from the Johns Hopkins Applied Physics Laboratory, and
Don Yeomans, from the Jet Propulsion Laboratory, also contributed
detailed and interesting aspects of the Trojan asteroids for scientific
prioritization.
NR 19
TC 0
Z9 0
U1 2
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR
PY 2016
VL 53
IS 2
BP 278
EP 288
DI 10.2514/1.A33396
PG 11
WC Engineering, Aerospace
SC Engineering
GA DJ4IS
UT WOS:000374169200004
ER
PT J
AU Mason, JP
Woods, TN
Caspi, A
Chamberlin, PC
Moore, C
Jones, A
Kohnert, R
Li, XL
Palo, S
Solomon, SC
AF Mason, James P.
Woods, Thomas N.
Caspi, Amir
Chamberlin, Phillip C.
Moore, Christopher
Jones, Andrew
Kohnert, Rick
Li, Xinlin
Palo, Scott
Solomon, Stanley C.
TI Miniature X-Ray Solar Spectrometer: A Science-Oriented, University 3U
CubeSat
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID PHOTOMETER SYSTEM XPS; RELATIVISTIC ELECTRONS; ATOMIC DATABASE;
EMISSION-LINES; IRRADIANCE; CHIANTI; FLARES; CALIBRATIONS; RHESSI; BELT
AB The miniature x-ray solar spectrometer is a three-unit CubeSat developed at the Laboratory for Atmospheric and Space Physics at the University of Colorado, Boulder. Over 40 students contributed to the project with professional mentorship and technical contributions from professors in the Aerospace Engineering Sciences Department at University of Colorado, Boulder and from Laboratory for Atmospheric and Space Physics scientists and engineers. The scientific objective of the miniature x-ray solar spectrometer is to study processes in the dynamic sun, from quiet sun to solar flares, and to further understand how these changes in the sun influence the Earth's atmosphere by providing unique spectral measurements of solar soft x rays. The enabling technology providing the advanced solar soft x-ray spectral measurements is the Amptek X123, a commercial off-the-shelf silicon drift detector. The Amptek X123 has a low mass (similar to 324g after modification), modest power consumption (similar to 2.50W), and small volume (6.86x9.91x2.54cm), making it ideal for a CubeSat. This paper provides an overview of the miniature x-ray solar spectrometer mission: the science objectives, project history, subsystems, and lessons learned, which can be useful for the small-satellite community.
C1 [Mason, James P.] Univ Colorado, Lab Atmospher & Space Phys, Aerosp Engn Sci, 3665 Discovery Dr, Boulder, CO 80303 USA.
[Woods, Thomas N.] Univ Colorado, Lab Atmospher & Space Phys, Tech Div, 3665 Discovery Dr, Boulder, CO 80303 USA.
[Caspi, Amir] SW Res Inst, Dept Space Studies, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA.
[Chamberlin, Phillip C.] NASA, Goddard Space Flight Ctr, Heliophys Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Moore, Christopher] Univ Colorado, Lab Atmospher & Space Phys, Astrophys & Planetary Sci, 429 UCB, Boulder, CO 80303 USA.
[Jones, Andrew; Kohnert, Rick] Univ Colorado, Lab Atmospher & Space Phys, 3665 Discovery Dr, Boulder, CO 80303 USA.
[Li, Xinlin] Univ Colorado, Lab Atmospher & Space Phys, Aerosp Engn Sci, 429 UCB, Boulder, CO 80303 USA.
[Palo, Scott] Univ Colorado, Aerosp Engn Sci, 429 UCB, Boulder, CO 80303 USA.
[Solomon, Stanley C.] Natl Ctr Atmospher Res, High Altitude Observ, 3090 Ctr Green Dr, Boulder, CO 80301 USA.
RP Mason, JP (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Aerosp Engn Sci, 3665 Discovery Dr, Boulder, CO 80303 USA.
RI Chamberlin, Phillip/C-9531-2012; Solomon, Stanley/J-4847-2012;
OI Chamberlin, Phillip/0000-0003-4372-7405; Solomon,
Stanley/0000-0002-5291-3034; Caspi, Amir/0000-0001-8702-8273
FU NASA [NNX14AN84G]; National Science Foundation [AGSW0940277]; University
of Colorado at Boulder Aerospace Engineering Sciences department
FX This work was supported by NASA grant NNX14AN84G and National Science
Foundation grant AGSW0940277, as well as the University of Colorado at
Boulder Aerospace Engineering Sciences department. We would like to
specially thank the many professional scientists and engineers that
provided feedback at reviews and mentorship to students.
NR 44
TC 4
Z9 4
U1 4
U2 4
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR
PY 2016
VL 53
IS 2
BP 328
EP 339
DI 10.2514/1.A33351
PG 12
WC Engineering, Aerospace
SC Engineering
GA DJ4IS
UT WOS:000374169200008
ER
PT J
AU Mehta, U
Aftosmis, M
Bowles, J
Pandya, S
AF Mehta, Unmeel
Aftosmis, Michael
Bowles, Jeffrey
Pandya, Shishir
TI Skylon Aerospace Plane and Its Aerodynamics and Plumes
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID SPACEPLANE
AB The Skylon concept incorporates the highly innovative synergetic air-breathing rocket engine concept that has the potential to revolutionize the mode of propulsion for transportation of medium-weight payloads to low Earth orbits. An independent partial assessment is provided of the technical viability of the Skylon concept. Pressure lift and drag coefficients derived from Euler simulations for unpowered flight compare very well and fairly well, respectively, with those from engineering methods. The engineering-method coefficients for powered flight are increasingly less acceptable as the freestream Mach number is increased beyond 8.5 because these methods did not account for the increasing favorable (in terms of pressure forces) effect of underexpanded rocket engine plumes on the aft fuselage. At Mach numbers greater than 8.5, the thermal environment around the aft fuselage is a known unknown: a potential design and/or performance risk issue. The adverse effects of shock waves on the aft fuselage and plume-induced flow separation are other potential risks. A preliminary design of Skylon requires the judicious use of a combination of engineering methods, advanced methods based on required physics or analytical fidelity, test data, and independent assessments. The demonstration of a synergetic air-breathing rocket-engine-powered experimental aerospace plane calls for the second revival of the Aerospace Plane Program.
C1 [Mehta, Unmeel] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA.
[Aftosmis, Michael] NASA, Ames Res Ctr, Appl Modeling & Simulat Branch, Moffett Field, CA 94035 USA.
[Bowles, Jeffrey] NASA, Ames Res Ctr, Syst Anal Branch, Moffett Field, CA 94035 USA.
[Pandya, Shishir] NASA, Ames Res Ctr, Fundamental Modeling & Simulat Branch, Moffett Field, CA 94035 USA.
RP Mehta, U (reprint author), NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA.; Aftosmis, M (reprint author), NASA, Ames Res Ctr, Appl Modeling & Simulat Branch, Moffett Field, CA 94035 USA.; Bowles, J (reprint author), NASA, Ames Res Ctr, Syst Anal Branch, Moffett Field, CA 94035 USA.; Pandya, S (reprint author), NASA, Ames Res Ctr, Fundamental Modeling & Simulat Branch, Moffett Field, CA 94035 USA.
EM Unmeel.B.Mehta@nasa.gov; Michael.Aftosmis@nasa.gov;
Jeffrey.V.Bowles@nasa.gov; Shishir.Pandya@nasa.gov
NR 63
TC 0
Z9 0
U1 9
U2 9
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAR
PY 2016
VL 53
IS 2
BP 340
EP 353
DI 10.2514/1.A33408
PG 14
WC Engineering, Aerospace
SC Engineering
GA DJ4IS
UT WOS:000374169200009
ER
PT J
AU Fok, CL
Johnson, G
Yamokoski, JD
Mok, A
Sentis, L
AF Fok, Chien-Liang
Johnson, Gwendolyn
Yamokoski, John D.
Mok, Aloysius
Sentis, Luis
TI ControlIt! A Software Framework for Whole-Body Operational Space Control
SO INTERNATIONAL JOURNAL OF HUMANOID ROBOTICS
LA English
DT Article
DE Software framework; whole-body control; whole-body operational space
control; upperbody humanoid robot
ID INVERSE-DYNAMICS CONTROL; HUMANOID-ROBOT; FORCE CONTROL; MOTION
GENERATION; UNIFIED APPROACH; SYSTEM; MANIPULATION; ARCHITECTURE;
CONSTRAINTS
AB Whole Body Operational Space Control (WBOSC) enables floating-base highly redundant robots to achieve unified motion/force control of one or more operational space objectives while adhering to physical constraints. It is a pioneering algorithm in the field of human-centered Whole-Body Control (WBC). Although there are extensive studies on the algorithms and theory behind WBOSC, limited studies exist on the software architecture and APIs that enable WBOSC to perform and be integrated into a larger system. In this paper, we address this by presenting ControlIt!, a new open-source software framework for WBOSC. Unlike previous implementations, ControlIt! is multi-threaded to increase maximum servo frequencies using standard PC hardware. Anew parameter binding mechanism enables tight integration between ControlIt! and external processes via an extensible set of transport protocols. To support a new robot, only two plugins and a URDF model is needed - the rest of ControlIt! remains unchanged. New WBC primitives can be added by writing Task or Constraint plugins. ControlIt!'s capabilities are demonstrated on Dreamer, a 16-DOF torque controlled humanoid upper body robot containing both series elastic and co-actuated joints, and using it to perform a product disassembly task. Using this testbed, we show that ControlIt! can achieve average servo latencies of about 0.5 ms when con figured with two Cartesian position tasks, two orientation tasks, and a lower priority posture task. This is 10 times faster than the 5 ms that was achieved using UTA-WBC, the prototype implementation of WBOSC that is both application and platform-specific. Variations in the product's position is handled by updating the goal of the Cartesian position task. ControlIt!'s source code is released under LGPL and we hope it will be adopted and maintained by the WBC community for the long term as a platform for WBC development and integration.
C1 [Fok, Chien-Liang; Johnson, Gwendolyn; Sentis, Luis] Univ Texas Austin, Mech Engn, Human Ctr Robot Lab, 204 East Dean Keeton St, Austin, TX 78712 USA.
[Fok, Chien-Liang; Yamokoski, John D.] NASA, Lyndon B Johnson Space Ctr, 2101 NASA Rd 1, Houston, TX 77058 USA.
[Mok, Aloysius] Univ Texas Austin, Comp Sci, UT Real Time Syst Grp, 2317 Speedway,Stop D9500, Austin, TX 78712 USA.
RP Fok, CL; Johnson, G; Sentis, L (reprint author), Univ Texas Austin, Mech Engn, Human Ctr Robot Lab, 204 East Dean Keeton St, Austin, TX 78712 USA.; Fok, CL; Yamokoski, JD (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Rd 1, Houston, TX 77058 USA.; Mok, A (reprint author), Univ Texas Austin, Comp Sci, UT Real Time Syst Grp, 2317 Speedway,Stop D9500, Austin, TX 78712 USA.
EM liangfok@gmail.com; gwendolynbrook@gmail.com; john.d.yamokoski@nasa.gov;
mok@cs.utexas.edu; 1sentis@austin.utexas.edu
FU NASA [NNX12AQ99G]; NSF NRI grant [NNX12AM03G]; ONR grant
[N000141210663]; Texas Emerging Technology Fund
FX We would like to thank the entire 2013 NASA Johnson Space Center DARPA
Robotics Challenge team for helping with the integration, testing, and
usage of ControlIt! on Valkyrie. This work is funded in part by NASA
grant #NNX12AQ99G, NSF NRI grant #NNX12AM03G, ONR grant #N000141210663,
Texas Emerging Technology Fund, and an anonymous donor. We would also
like to thank Nicholas Paine for helping with some figures in the
evaluation section.
NR 124
TC 1
Z9 1
U1 0
U2 2
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE
SN 0219-8436
EI 1793-6942
J9 INT J HUM ROBOT
JI Int. J. Humanoid Robot.
PD MAR
PY 2016
VL 13
IS 1
SI SI
AR 1550040
DI 10.1142/S0219843615500401
PG 57
WC Robotics
SC Robotics
GA DJ2CR
UT WOS:000374011800003
ER
PT J
AU Gupta, KK
Choi, SB
Ibrahim, H
AF Gupta, K. K.
Choi, S. B.
Ibrahim, H.
TI Development-Fluid-Dynamics-Based Aerothermoelastic Simulation Capability
with Application to Flight Vehicles
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID AEROELASTIC ANALYSIS; HYPERSONIC FLOW; EULER; FUTURE; MESH
AB Aerodynamic heating on structural surfaces plays an important role in the aeroelastic stability of flight vehicles, particularly in a high-temperature environment. The thermal effects of high-speed flow, obtained from a heat-conduction analysis, at the end of an unsteady time step are incorporated in the model solution, which in turn affects the unsteady flow arising out of interaction of the elastic structure with the air. This paper describes the development, implementation, and application of a highly integrated computational-fluid-dynamics-based aerothermoelastic analysis capability and the resulting code. The associated methodology employs the common finite element discretization for both fluid and structure disciplines using unstructured grids. An aeroelastic matrix formulation that uses a transpiration technique in lieu of aerodynamics mesh updating affects an efficient and accurate simulation of the aerothermoelastic phenomenon. The first example problem of a cantilever wing demonstrates the possible severity of thermal effects on a flutter mechanism. The second example of the X-43 hypersonic flight vehicle shows that the current procedure and the code can effectively solve complex practical problems with moderate computational resources. The accuracy and relative efficiency of the computational-fluid-dynamics and structural solutions are verified using actual flight and ground vibration tests.
C1 [Gupta, K. K.] NASA, Armstrong Flight Res Ctr, Res Engn Directorate, Edwards AFB, CA 93523 USA.
[Choi, S. B.] Calif State Univ Los Angeles, Dept Mech Engn, Los Angeles, CA 90032 USA.
[Ibrahim, H.] Norfolk State Univ, Dept Engn, Norfolk, VA 23504 USA.
RP Gupta, KK (reprint author), NASA, Armstrong Flight Res Ctr, Res Engn Directorate, Edwards AFB, CA 93523 USA.
NR 18
TC 0
Z9 0
U1 2
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2016
VL 53
IS 2
BP 360
EP 368
DI 10.2514/1.C033346
PG 9
WC Engineering, Aerospace
SC Engineering
GA DJ1EC
UT WOS:000373945100006
ER
PT J
AU Broeren, AP
Lee, S
Clark, C
AF Broeren, Andy P.
Lee, Sam
Clark, Catherine
TI Aerodynamic Effects of Anti-Icing Fluids on a Thin High-Performance Wing
Section
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 5th AIAA Atmospheric and Space Environments Conference
CY JUN 24-27, 2013
CL San Diego, CA
SP AIAA
ID LEADING-EDGE; ICE ACCRETIONS; SEPARATION
AB The Federal Aviation Administration has worked with Transport Canada and others to develop allowance times for aircraft operating in ice-pellet precipitation based upon wind-tunnel experiments with a thin high-performance wing. These allowance times are applicable to many different airplanes. Therefore, the aim of this work is to characterize the aerodynamic behavior of the wing section in order to better understand the adverse aerodynamic effects of anti-icing fluids and ice-pellet contamination. Aerodynamic performance tests, boundary-layer surveys, and flow visualization were conducted at a Reynolds number of approximately 6.0x106 and a Mach number of 0.12. Roughness and leading-edge flow disturbances were employed to simulate the aerodynamic impact of the anti-icing fluids and contamination. In the linear portion of the lift curve, the primary aerodynamic effect is the thickening of the downstream boundary layer due to the accumulation of fluid and contamination. This causes a reduction in lift coefficient and an increase in pitching moment (nose up) due to an effective decambering of the wing. The stalling characteristics of the wing with fluid and contamination appear to be driven at least partially by the effects of a secondary wave of fluid that forms near the leading edge as the wing is rotated in the simulated takeoff profile. These results have provided a much more complete understanding of the adverse aerodynamic effects of anti-icing fluids and ice-pellet contamination on this wing.
C1 [Broeren, Andy P.] NASA, John H Glenn Res Ctr, Icing Branch, 21000 Brookpark Rd,MS 11-2, Cleveland, OH 44135 USA.
[Lee, Sam] Vantage Partners LLC, Icing Branch, 21000 Brookpark Rd,MS 11-2, Cleveland, OH 44135 USA.
[Clark, Catherine] Natl Res Council Canada, Aerosp Portfolio, 1200 Montreal Rd,Bldg U-66, Ottawa, ON K1A 0R6, Canada.
RP Broeren, AP (reprint author), NASA, John H Glenn Res Ctr, Icing Branch, 21000 Brookpark Rd,MS 11-2, Cleveland, OH 44135 USA.
NR 29
TC 0
Z9 0
U1 5
U2 7
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2016
VL 53
IS 2
BP 451
EP 462
DI 10.2514/1.C033384
PG 12
WC Engineering, Aerospace
SC Engineering
GA DJ1EC
UT WOS:000373945100015
ER
PT J
AU Park, MA
Morgenstern, JM
AF Park, Michael A.
Morgenstern, John M.
TI Summary and Statistical Analysis of the First AIAA Sonic Boom Prediction
Workshop
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 32nd AIAA Applied Aerodynamics Conference
CY JUN 16-20, 2014
CL Atlanta, GA
SP AIAA
ID COMPUTATIONAL FLUID-DYNAMICS; AIRCRAFT; NASA
AB A summary is provided for the First AIAA Sonic Boom Workshop held 11January2014 in conjunction with AIAA SciTech 2014. Near-field pressure signatures extracted from computational-fluid-dynamics solutions are gathered from 19 participants (representing three countries) for the two required cases: an axisymmetric body and a simple delta-wing configuration. Structured multiblock, unstructured mixed-element, unstructured tetrahedral, overset, and Cartesian cut-cell methods are used by the participants. Participants provided signatures computed on a series of uniformly refined workshop provided grids and participant-generated and solution-adapted grids. These submissions are propagated to the ground, and noise measures are computed. This allows the grid convergence of a noise measure and a validation metric (difference norm between computed and wind-tunnel-measured near-field signatures) to be studied for the first time. A statistical analysis is also presented for these measures. An optional configuration includes fuselage, wing, tail, flow-through nacelles, and blade sting. More variation in computed noise measures are observed for this full configuration than the required cases. Recommendations are provided for potential improvements to the analysis methods and a possible subsequent workshop.
C1 [Park, Michael A.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
[Morgenstern, John M.] Lockheed Martin Aeronaut Co, Adv Dev Programs, Palmdale, CA 93599 USA.
RP Park, MA (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
NR 58
TC 1
Z9 1
U1 1
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD MAR-APR
PY 2016
VL 53
IS 2
BP 578
EP 598
DI 10.2514/1.C033449
PG 21
WC Engineering, Aerospace
SC Engineering
GA DJ1EC
UT WOS:000373945100024
ER
PT J
AU Cantu, LML
Gallo, ECA
Cutler, AD
Bathel, BF
Danehy, PM
Rockwell, RD
Goyne, CP
McDaniel, JC
AF Cantu, Luca M. L.
Gallo, Emanuela C. A.
Cutler, Andrew D.
Bathel, Brett F.
Danehy, Paul M.
Rockwell, Robert D.
Goyne, Christopher P.
McDaniel, James C.
TI Visualization of Simulated Fuel-Air Mixing in a Dual-Mode Scramjet
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article; Proceedings Paper
CT 53rd AIAA Aerospace Sciences Meeting
CY JAN 05-09, 2015
CL Kissimmee, FL
SP AIAA
ID LASER-INDUCED FLUORESCENCE; INDUCED IODINE FLUORESCENCE; INJECTANT
MOLE-FRACTION; SUPERSONIC CROSS-FLOW; NO; COMBUSTION; FLOWFIELD; SYSTEM
AB Nitric oxide planar laser-induced fluorescence measurements have been performed in a small-scale scramjet combustor at the University of Virginia Aerospace Research Laboratory at nominal simulated Mach 5 flight. A mixture of nitric oxide and nitrogen was injected at the upstream end of the inlet isolator as a surrogate for ethylene fuel, and the mixing of this fuel simulant was studied with and without a shock train. The shock train was produced by an air throttle, which simulated the blockage effects of combustion downstream of the cavity flameholder. Nitric oxide planar laser-induced fluorescence signal was imaged in a plane orthogonal to the freestream at the leading edge of the cavity. Instantaneous planar images were recorded and analyzed to identify the most uniform cases, which were achieved by varying the location of the fuel injection and shock train. This method was used to screen different possible fueling configurations to provide optimized test conditions for follow-on combustion measurements using ethylene fuel. A theoretical study of the selected nitric oxide rotational transitions was performed to obtain a laser-induced fluorescence signal that was linear with the nitric oxide mole fraction and approximately independent of the pressure and temperature.
C1 [Cantu, Luca M. L.; Gallo, Emanuela C. A.; Cutler, Andrew D.] George Washington Univ, Mech & Aerosp Engn, Washington, DC 20052 USA.
[Bathel, Brett F.; Danehy, Paul M.] NASA, Langley Res Ctr, Adv Measurements & Data Syst Branch, MS 493, Hampton, VA 23681 USA.
[Rockwell, Robert D.; Goyne, Christopher P.; McDaniel, James C.] Univ Virginia, Mech & Aerosp Engn, Charlottesville, VA 22904 USA.
RP Cantu, LML (reprint author), George Washington Univ, Mech & Aerosp Engn, Washington, DC 20052 USA.
NR 55
TC 1
Z9 1
U1 1
U2 10
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
EI 1533-3876
J9 J PROPUL POWER
JI J. Propul. Power
PD MAR
PY 2016
VL 32
IS 2
BP 373
EP 382
DI 10.2514/1.B35760
PG 10
WC Engineering, Aerospace
SC Engineering
GA DJ0YR
UT WOS:000373930800011
ER
PT J
AU Heath, CM
AF Heath, Christopher M.
TI Parametric Modeling Investigation for Radially Staged Low-Emission
Combustion
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
AB Aviation gas-turbine combustion demands high efficiency, wide operability, and minimal trace gas emissions. Performance critical design parameters include injector geometry, combustor layout, fuel-air mixing, and engine cycle conditions. The present investigation explores these factors and their impact on a radially staged low-emission aviation combustor sized for a next-generation 24,000-lbf-thrust engine. By coupling multifidelity computational tools, a design exploration was performed using a parameterized annular combustor sector at projected 100% takeoff power conditions. Design objectives included nitrogen oxide emission indices and overall combustor pressure loss. From the design space, an optimal configuration was selected and simulated at 7.1, 30, and 85% part-power operation, corresponding to landing-takeoff cycle idle, approach, and climb segments. All results were obtained by solution of the steady-state Reynolds-averaged Navier-Stokes equations. Species concentrations were solved directly using a reduced 19-step reaction mechanism for Jet A. Turbulence closure was obtained using a nonlinear -E model. This research demonstrates revolutionary combustor design exploration enabled by multifidelity physics-based simulation.
C1 [Heath, Christopher M.] NASA, John H Glenn Res Ctr, Prop Syst Anal Branch, MS 5-10, Cleveland, OH 44135 USA.
RP Heath, CM (reprint author), NASA, John H Glenn Res Ctr, Prop Syst Anal Branch, MS 5-10, Cleveland, OH 44135 USA.
FU NASA
FX The author gratefully acknowledges the Commercial Supersonic Technology
and AeroSciences Projects of the NASA Fundamental Aeronautics Program
for research funding. Acknowledgment is also due to PhilLee of Woodward
Fuel Systems Textron, Inc., for providing general injector design
guidelines and Thomas Wey of NASA Glenn Research Center for technical
OpenNCC solver support.
NR 31
TC 0
Z9 0
U1 1
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
EI 1533-3876
J9 J PROPUL POWER
JI J. Propul. Power
PD MAR
PY 2016
VL 32
IS 2
BP 500
EP 515
DI 10.2514/1.B35867
PG 16
WC Engineering, Aerospace
SC Engineering
GA DJ0YR
UT WOS:000373930800023
ER
PT J
AU Kelley, C
France, S
Parrish, F
Wagner, D
Gerringer, M
Garcia, M
AF Kelley, Christopher
France, Scott
Parrish, Frank
Wagner, Daniel
Gerringer, Mackenzie
Garcia, Michael
TI CAPSTONE's First Year-2015 Hohonu Moana: Exploring Deep Waters off
Hawai'i
SO OCEANOGRAPHY
LA English
DT Editorial Material
C1 [Kelley, Christopher] Univ Hawaii, Hawaii Undersea Res Lab, Honolulu, HI 96822 USA.
[France, Scott] Univ Louisiana Lafayette, Biol, Lafayette, LA 70504 USA.
[Parrish, Frank] NOAA, Protected Species Div, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI USA.
[Wagner, Daniel] NOAA, Papahanaumokuakea Marine Natl Monument, Honolulu, HI USA.
[Gerringer, Mackenzie] Univ Hawaii, Honolulu, HI 96822 USA.
[Garcia, Michael] Univ Hawaii, Dept Geol & Geophys, Geol, Honolulu, HI 96822 USA.
RP Kelley, C (reprint author), Univ Hawaii, Hawaii Undersea Res Lab, Honolulu, HI 96822 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD MAR
PY 2016
VL 29
IS 1
SU S
BP 68
EP 73
PG 6
WC Oceanography
SC Oceanography
GA DJ3IM
UT WOS:000374098100020
ER
PT J
AU Keener, P
Crum, E
Hirsh, H
AF Keener, Paula
Crum, Emily
Hirsh, Heidi
TI Okeanos Explorer Engages Far and Wide in 2015
SO OCEANOGRAPHY
LA English
DT Editorial Material
C1 [Keener, Paula] NOAA, Educ, Off Ocean Explorat & Res, Charleston, SC USA.
[Crum, Emily] NOAA, Off Ocean Explorat & Res, Key West, FL USA.
[Hirsh, Heidi] NOAA, Natl Marine Fisheries Serv, Pacific Isl Reg Off, Marine Natl Monument Program, Honolulu, HI USA.
RP Keener, P (reprint author), NOAA, Educ, Off Ocean Explorat & Res, Charleston, SC USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD MAR
PY 2016
VL 29
IS 1
SU S
BP 74
EP 75
PG 2
WC Oceanography
SC Oceanography
GA DJ3IM
UT WOS:000374098100021
ER
PT J
AU Lindstrom, E
Hakkinen, S
Wei, MY
AF Lindstrom, Eric
Hakkinen, Sirpa
Wei, Ming-Ying
TI NASA Graduate Fellowship Opportunities
SO OCEANOGRAPHY
LA English
DT Article
AB The US National Aeronautics and Space Administration (NASA) has a robust program in Earth observing and Earth science research, including oceanography. For decades, the agency has supported graduate students through research grants and a dedicated graduate fellowship program. The core and the longest-active graduate student program is the NASA Earth and Space Science Fellowship geared to students in basic and applied research in Earth and space science. This article provides some history and context for NASA's investment in oceanography graduate students, along with testimonials from some graduate fellowship recipients.
C1 [Lindstrom, Eric] NASA, Phys Oceanog Res Program, NASA Headquarters, Greenbelt, MD USA.
[Lindstrom, Eric] Steering Comm Global Ocean Observing Syst, Barcelona, Spain.
[Hakkinen, Sirpa] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Wei, Ming-Ying] NASA, Earth Sci Educ Programs, Greenbelt, MD USA.
RP Lindstrom, E (reprint author), NASA, Phys Oceanog Res Program, NASA Headquarters, Greenbelt, MD USA.; Lindstrom, E (reprint author), Steering Comm Global Ocean Observing Syst, Barcelona, Spain.
EM eric.j.lindstrom@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD MAR
PY 2016
VL 29
IS 1
SI SI
BP 82
EP 85
DI 10.5670/oceanog.2016.19
PG 4
WC Oceanography
SC Oceanography
GA DJ3IJ
UT WOS:000374097800019
ER
PT J
AU Uz, SS
AF Uz, Stephanie Schollaert
TI Building Intuition for In-Water Optics and Ocean Color Remote Sensing
Spectrophotometer Activity with littleBits (TM)
SO OCEANOGRAPHY
LA English
DT Editorial Material
C1 [Uz, Stephanie Schollaert] Global Sci & Technol Inc, New Ocean Color Satellite Mission, PACE, Greenbelt, MD USA.
[Uz, Stephanie Schollaert] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD USA.
RP Uz, SS (reprint author), Global Sci & Technol Inc, New Ocean Color Satellite Mission, PACE, Greenbelt, MD USA.; Uz, SS (reprint author), NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD USA.
EM stephanie.uz@nasa.gov
NR 1
TC 0
Z9 0
U1 3
U2 3
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD MAR
PY 2016
VL 29
IS 1
SI SI
BP 98
EP 103
DI 10.5670/oceanog.2016.01
PG 6
WC Oceanography
SC Oceanography
GA DJ3IJ
UT WOS:000374097800022
ER
PT J
AU Claverie, M
Matthews, JL
Vermote, EF
Justice, CO
AF Claverie, Martin
Matthews, Jessica L.
Vermote, Eric F.
Justice, Christopher O.
TI A 30+ Year AVHRR LAI and FAPAR Climate Data Record: Algorithm
Description and Validation
SO REMOTE SENSING
LA English
DT Article
DE AVHRR; LAI; climate data record; land product validation; MODIS; FAPAR
ID LEAF-AREA INDEX; PHOTOSYNTHETICALLY ACTIVE RADIATION; CYCLOPES GLOBAL
PRODUCTS; TIME-SERIES; VEGETATION CANOPY; IN-SITU; PART 2; MODIS;
REFLECTANCE; FRACTION
AB In- land surface models, which are used to evaluate the role of vegetation in the context of global climate change and variability, LAI and FAPAR play a key role, specifically with respect to the carbon and water cycles. The AVHRR-based LAI/FAPAR dataset offers daily temporal resolution, an improvement over previous products. This climate data record is based on a carefully calibrated and corrected land surface reflectance dataset to provide a high-quality, consistent time-series suitable for climate studies. It spans from mid-1981 to the present. Further, this operational dataset is available in near real-time allowing use for monitoring purposes. The algorithm relies on artificial neural networks calibrated using the MODIS LAI/FAPAR dataset. Evaluation based on cross-comparison with MODIS products and in situ data show the dataset is consistent and reliable with overall uncertainties of 1.03 and 0.15 for LAI and FAPAR, respectively. However, a clear saturation effect is observed in the broadleaf forest biomes with high LAI (>4.5) and FAPAR (>0.8) values.
C1 [Claverie, Martin; Justice, Christopher O.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Claverie, Martin; Vermote, Eric F.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Matthews, Jessica L.] NOAAs, NCEI, 151 Patton Ave, Asheville, NC 28801 USA.
[Matthews, Jessica L.] N Carolina State Univ, CICS NC, 151 Patton Ave, Asheville, NC 28801 USA.
RP Claverie, M (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.; Claverie, M (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM mcl@umd.edu
OI Matthews, Jessica L./0000-0002-6968-3474
FU NOAA through the Cooperative Institute for Climate and Satellites -
North Carolina [NA14NES432003]
FX The authors would like to acknowledge NOAA NCEI for supporting the
development of the AVH15 product. J. L. M. was supported by NOAA through
the Cooperative Institute for Climate and Satellites - North Carolina
under Cooperative Agreement NA14NES432003.
NR 32
TC 2
Z9 2
U1 5
U2 11
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD MAR
PY 2016
VL 8
IS 3
DI 10.3390/rs8030263
PG 12
WC Remote Sensing
SC Remote Sensing
GA DI6RJ
UT WOS:000373627400008
ER
PT J
AU Loeb, NG
Manalo-Smith, N
Su, WY
Shankar, M
Thomas, S
AF Loeb, Norman G.
Manalo-Smith, Natividad
Su, Wenying
Shankar, Mohan
Thomas, Susan
TI CERES Top-of-Atmosphere Earth Radiation Budget Climate Data Record:
Accounting for in-Orbit Changes in Instrument Calibration
SO REMOTE SENSING
LA English
DT Article
DE climate; satellite; calibration; earth radiation budget; radiance
ID ENERGY SYSTEM CERES; ANGULAR-DISTRIBUTION MODELS; RAINFALL MEASURING
MISSION; TERRA SATELLITE; FLUX ESTIMATION; CLOUDS; SPACECRAFT;
METHODOLOGY; VALIDATION; RADIANCES
AB The Clouds and the Earth's Radiant Energy System (CERES) project provides observations of Earth's radiation budget using measurements from CERES instruments onboard the Terra, Aqua and Suomi National Polar-orbiting Partnership (S-NPP) satellites. As the objective is to create a long-term climate data record, it is necessary to periodically reprocess the data in order to incorporate the latest calibration changes and algorithm improvements. Here, we focus on the improvements and validation of CERES Terra and Aqua radiances in Edition 4, which are used to generate higher-level climate data products. Onboard sources indicate that the total (TOT) channel response to longwave (LW) radiation has increased relative to the start of the missions by 0.4% to 1%. In the shortwave (SW), the sensor response change ranges from -0.4% to 0.6%. To account for in-orbit changes in SW spectral response function (SRF), direct nadir radiance comparisons between instrument pairs on the same satellite are made and an improved wavelength dependent degradation model is used to adjust the SRF of the instrument operating in a rotating azimuth plane scan mode. After applying SRF corrections independently to CERES Terra and Aqua, monthly variations amongst these instruments are highly correlated and the standard deviation in the difference of monthly anomalies is 0.2 Wm(-2) for ocean and 0.3 Wm(-2) for land/desert. Additionally, trends in CERES Terra and Aqua monthly anomalies are consistent to 0.21 Wm(-2) per decade for ocean and 0.31 Wm(-2) per decade for land/desert. In the LW, adjustments to the TOT channel SRF are made to ensure that removal of the contribution from the SW portion of the TOT channel with SW channel radiance measurements during daytime is consistent throughout the mission. Accordingly, anomalies in day-night LW difference in Edition 4 are more consistent compared to Edition 3, particularly for the Aqua land/desert case.
C1 [Loeb, Norman G.; Su, Wenying] NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
[Manalo-Smith, Natividad; Shankar, Mohan; Thomas, Susan] Sci Syst & Applicat Inc, 1 Enterprise Pkwy 200, Hampton, VA 23666 USA.
RP Loeb, NG (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM norman.g.loeb@nasa.gov; nitchie.smith@nasa.gov; wenying.su-1@nasa.gov;
mohan.shankar-1@nasa.gov; susan.thomas-1@nasa.gov
FU NASA CERES project
FX This research has been supported by the NASA CERES project. The CERES
datasets were obtained from http://ceres.larc.nasa.gov/order_data.php.
The NASA Langley Atmospheric Sciences Data Center processed the
instantaneous Single Scanner Footprint data used in this analysis.
NR 22
TC 0
Z9 0
U1 4
U2 9
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD MAR
PY 2016
VL 8
IS 3
DI 10.3390/rs8030182
PG 14
WC Remote Sensing
SC Remote Sensing
GA DI6RJ
UT WOS:000373627400094
ER
PT J
AU Bergvall, N
Marquart, T
Way, MJ
Blomqvist, A
Holst, E
Ostlin, G
Zackrisson, E
AF Bergvall, Nils
Marquart, Thomas
Way, Michael J.
Blomqvist, Anna
Holst, Emma
Ostlin, Goran
Zackrisson, Erik
TI Local starburst galaxies and their descendants Statistics from the Sloan
Digital Sky Survey
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: evolution; galaxies: luminosity function, mass function;
galaxies: starburst; galaxies: star formation; galaxies: statistics;
galaxies: stellar content
ID STAR-FORMING GALAXIES; BLUE COMPACT GALAXIES; EMISSION-LINE GALAXIES;
LYMAN BREAK GALAXIES; H-II REGIONS; ULTRALUMINOUS INFRARED GALAXIES;
SPECTROSCOPIC TARGET SELECTION; HIGH-REDSHIFT GALAXIES; ALPHA
VELOCITY-FIELDS; INITIAL MASS FUNCTION
AB Aims. Despite strong interest in the starburst phenomenon in extragalactic astronomy, the concept remains ill-defined. Here we use a strict definition of starburst to examine the statistical properties of starburst galaxies in the local universe. We also seek to establish links between starburst galaxies, post-starburst (hereafter postburst) galaxies, and active galaxies.
Methods. Data were selected from the Sloan Digital Sky Survey DR7. We applied a novel method of treating dust attenuation and derive star formation rates, ages, and stellar masses assuming a two-component stellar population model. Dynamical masses are calculated from the width of the H alpha line. These masses agree excellently with the photometric masses. The mass (gas + stars) range is similar to 10(9)-10(11.5) M-circle dot. As a selection criterion for starburst galaxies, we use, the birthrate parameter, b = SFR/< SFR >, requiring that b >= 3. For postburst galaxies, we use, the equivalent width of H delta in absorption with the criterion EWH delta,abs >= 6 angstrom.
Results. We find that only 1% of star-forming galaxies are starburst galaxies. They contribute 3 6% to the stellar production and are therefore unimportant for the local star formation activity. The median starburst age is 70 Myr roughly independent of mass, indicating that star formation is mainly regulated by local feedback processes. The b-parameter strongly depends on burst age. Values close to b = 60 are found at ages similar to 10 Myr, while almost no starbursts are found at ages >1 Gyr. The median baryonic burst mass fraction of sub-L* galaxies is 5% and decreases slowly towards high masses. The median mass fraction of the recent burst in the postburst sample is 5-10%. A smaller fraction of the postburst galaxies, however, originates in non-bursting galaxies. The age-mass distribution of the postburst progenitors (with mass fractions >3%) is bimodal with a break at log M (M-circle dot) similar to 10.6, above which the ages are doubled. The starburst and postburst luminosity functions (LFs) follow each other closely until M-r similar to -21, when active galactic nuclei (AGNs) begin to dominate. The postburst LF continues to follow the AGN LF, while starbursts become less significant. This suggests that the number of luminous starbursts is underestimated by about one dex at high luminosities, because of having large amounts of dust and/or being outshone by an AGN. It also indicates that the starburst phase preceded the AGN phase. Finally, we look at the conditions for global gas outflow caused by stellar feedback and find that massive starburst galaxies are susceptible to such outflows.
C1 [Bergvall, Nils; Marquart, Thomas; Way, Michael J.; Blomqvist, Anna; Holst, Emma; Zackrisson, Erik] Uppsala Univ, Dept Phys & Astron, Box 515, S-75120 Uppsala, Sweden.
[Way, Michael J.] NASA Goddard Inst Space Studies, 2880 Broadway, New York, NY 10029 USA.
[Ostlin, Goran] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden.
RP Bergvall, N (reprint author), Uppsala Univ, Dept Phys & Astron, Box 515, S-75120 Uppsala, Sweden.
EM nils.bergvall@astro.uu.se
OI Way, Michael/0000-0003-3728-0475
FU Swedish Research Council [2011-5349]; Wenner-Gren Foundations; Swedish
National Space Board; Alfred P. Sloan Foundation; National Aeronautics
and Space Administration; National Science Foundation; US Department of
Energy; Japanese Monbukagakusho; Max Planck Society
FX We are indebted to Dr. Polychronis Papaderos for stimulating discussions
and assisting us with the use of the STARLIGHT code and CAUP computer
facilities. The anonymous referee is thanked for useful comments on the
draft. E.Z. acknowledges research funding from the Swedish Research
Council (project 2011-5349), the Wenner-Gren Foundations and the Swedish
National Space Board. This research has made use of NASA's Astrophysics
Data System Bibliographic Services. Funding for the SDSS has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Aeronautics and Space Administration, the
National Science Foundation, the US Department of Energy, the Japanese
Monbukagakusho, and the Max Planck Society. The SDSS Web site is
http://www.sdss.org/. The SDSS is managed by the Astrophysical Research
Consortium for the Participating Institutions. The Participating
Institutions are The University of Chicago, Fermilab, the Institute for
Advanced Study, the Japan Participation Group, The Johns Hopkins
University, Los Alamos National Laboratory, the Max-Planck-Institute for
Astronomy, the Max-Planck-Institute for Astrophysics, New Mexico State
University, University of Pittsburgh, Princeton University, the United
States Naval Observatory, and the University of Washington.
NR 211
TC 2
Z9 2
U1 2
U2 8
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A72
DI 10.1051/0004-6361/201525692
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800083
ER
PT J
AU Chitta, LP
Peter, H
Young, PR
AF Chitta, L. P.
Peter, H.
Young, P. R.
TI A closer look at a coronal loop rooted in a sunspot umbra
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: corona; Sun: transition region; Sun: magnetic fields; techniques:
spectroscopic; line: profiles
ID REGION-IMAGING-SPECTROGRAPH; SOLAR TRANSITION REGION;
DYNAMICS-OBSERVATORY SDO; ACTIVE REGIONS; NONEQUILIBRIUM IONIZATION;
SPECTROSCOPIC OBSERVATIONS; ULTRAVIOLET-SPECTRA; ATOMIC DATABASE;
EMISSION-LINES; SIPHON FLOWS
AB Context. Extreme UV (EUV) and X-ray loops in the solar corona connect regions of enhanced magnetic activity, but they are not usually rooted in the dark umbrae of sunspots because the strong magnetic field found there suppresses convection. This means that the Poynting flux of magnetic energy into the upper atmosphere is not significant within the umbra as long as there are no light bridges or umbral dots.
Aims. Here we report a rare observation of a coronal loop rooted in the dark umbra of a sunspot without any traces of light bridges or umbral dots. This allows us to investigate the loop without much confusion from background or line-of-sight integration effects.
Methods. We used the slit-jaw images and spectroscopic data from the Interface Region Imaging Spectrograph (IRIS) and concentrate on the line profiles of O IV and Si IV that show persistent strong redshifted components in the loop rooted in the umbra. Using the ratios of O IV, we can estimate the density and thus investigate the mass flux. The coronal context and temperature diagnostics of these observations is provided through the EUV channels of the Atmospheric Imaging Assembly (AIA).
Results. The coronal loop, embedded within cooler downflows, hosts supersonic downflows. The speed of more than 100 km s(-1) is on the same order of magnitude in the transition region lines of OIV and Si IV, and is even seen at comparable speed in the chromospheric Mg II lines. At a projected distance of within 1 '' of the footpoint, we see a shock transition to smaller downflow speeds of about 15 km s(-1) being consistent with mass conservation across a stationary isothermal shock.
Conclusions. We see no direct evidence for energy input into the loop because the loop is rooted in the dark uniform part of the umbra with no light bridges or umbral dots near by. Thus one might conclude that we are seeing a siphon flow driven from the footpoint at the other end of the loop. However, for a final result data of similar quality at the other footpoint are needed, but this is too far away to be covered by the IRIS field of view.
C1 [Chitta, L. P.; Peter, H.] Max Planck Inst Solar Syst Res MPS, D-37077 Gottingen, Germany.
[Young, P. R.] George Mason Univ, Coll Sci, 4400 Univ Dr, Fairfax, VA 22030 USA.
[Young, P. R.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
RP Chitta, LP (reprint author), Max Planck Inst Solar Syst Res MPS, D-37077 Gottingen, Germany.
EM chitta@mps.mpg.de
OI Chitta, Lakshmi Pradeep/0000-0002-9270-6785
FU Max-Planck Princeton Center for Plasma Physics; NASA [NNX15AF48G]; ESA;
Norwegian Space Centre
FX The authors thank the anonymous referee for the constructive comments
and suggestions that helped improve the manuscript. L.P.C. acknowledges
funding by the Max-Planck Princeton Center for Plasma Physics. P.R.Y.
thanks the staff at the Max Planck Institute for Solar System Research
for their kind hospitality. Funding for P.R.Y. comes from NASA grant
NNX15AF48G. IRIS is a NASA small explorer mission developed and operated
by LMSAL with mission operations executed at NASA Ames Research center
and major contributions to downlink communications funded by ESA and the
Norwegian Space Centre. SDO data are the courtesy of NASA/SDO and the
AIA and HMI science teams. CHIANTI is a collaborative project involving
George Mason University, the University of Michigan (USA), and the
University of Cambridge (UK). This research has made use of NASA's
Astrophysics Data System.
NR 56
TC 1
Z9 1
U1 1
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A20
DI 10.1051/0004-6361/201527340
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800031
ER
PT J
AU Djupvik, AA
Liimets, T
Zinnecker, H
Barzdis, A
Rastorgueva-Foi, EA
Petersen, LR
AF Djupvik, A. A.
Liimets, T.
Zinnecker, H.
Barzdis, A.
Rastorgueva-Foi, E. A.
Petersen, L. R.
TI Proper motions of embedded protostellar jets in Serpens
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; ISM: jets and outflows; Herbig-Haro objects; ISM:
kinematics and dynamics
ID STAR-FORMING REGIONS; HERBIG-HARO OBJECTS; SPITZER C2D SURVEY;
MOLECULAR-HYDROGEN; AQUILA RIFT; YOUNG STARS; SPACE-TELESCOPE;
PROTOSTARS; EVOLUTION; EMISSION
AB Aims. We determine the proper motion of protostellar jets around Class 0 and Class I sources in an active star forming region in Serpens.
Methods. Multi-epoch deep images in the 2.122 mu m line of molecular hydrogen, v = 1-0 S(1), obtained with the near-infrared instrument NOTCam on a timescale of 10 years, are used to determine the proper motion of knots and jets. K-band spectroscopy of the brighter knots is used to supply radial velocities, estimate extinction, excitation temperature, and H-2 column densities towards these knots.
Results. We measure the proper motion of 31 knots on different timescales (2, 4, 6, 8, and 10 years). The typical tangential velocity is around 50 km s(-1) for the 10-year baseline, but for shorter timescales, a maximum tangential velocity up to 300 km s(-1) is found for a few knots. Based on morphology, velocity information, and the locations of known protostars, we argue for the existence of at least three partly overlapping and deeply embedded flows, one Class 0 flow and two Class I flows. The multi-epoch proper motion results indicate time-variable velocities of the knots, for the first time directly measured for a Class 0 jet. We find in general higher velocities for the Class 0 jet than for the two Class I jets. While the bolometric luminosites of the three driving sources are about equal, the derived mass flow rate (M) over dot(out) is two orders of magnitude higher in the Class 0 flow than in the two Class I flows.
C1 [Djupvik, A. A.] Nord Opt Telescope, Rambla Jose Ana Fernandez Perez 7, Brena Baja 38711, Spain.
[Liimets, T.] Tartu Observ, EE-61602 Toravere, Estonia.
[Liimets, T.] Univ Tartu, Inst Phys, Ravila 14c, EE-50411 Tartu, Estonia.
[Zinnecker, H.] NASA, Ames Res Ctr, SOFIA, Ctr Sci, Moffett Field, CA 94035 USA.
[Zinnecker, H.] Univ Stuttgart, Deutsch SOFIA Inst DSI, D-70569 Stuttgart, Germany.
[Barzdis, A.] Univ Latvia, Inst Astron, Raina Bulv 19, LV-1586 Riga, Latvia.
[Rastorgueva-Foi, E. A.] Univ Tasmania, Sch Maths & Phys, Hobart, Tas 7001, Australia.
[Petersen, L. R.] Univ Copenhagen, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark.
RP Djupvik, AA (reprint author), Nord Opt Telescope, Rambla Jose Ana Fernandez Perez 7, Brena Baja 38711, Spain.; Liimets, T (reprint author), Tartu Observ, EE-61602 Toravere, Estonia.; Liimets, T (reprint author), Univ Tartu, Inst Phys, Ravila 14c, EE-50411 Tartu, Estonia.; Zinnecker, H (reprint author), NASA, Ames Res Ctr, SOFIA, Ctr Sci, Moffett Field, CA 94035 USA.; Zinnecker, H (reprint author), Univ Stuttgart, Deutsch SOFIA Inst DSI, D-70569 Stuttgart, Germany.; Rastorgueva-Foi, EA (reprint author), Univ Tasmania, Sch Maths & Phys, Hobart, Tas 7001, Australia.
EM amanda@not.iac.es; tiina@obs.ee; hzinnecker@sofia.usra.edu;
efoi@utas.edu.au
FU NordForsk; European Commission [RI031675, 011892, 212104, 261541];
Estonian Ministry for Education and Science; European Social Fund's
Doctoral Studies and Internationalisation Programme DoRa; Kristjan Jaak
Scholarship
FX We thank the anonymous referee for suggestions that led to a substantial
improvement of the article. A.A.D. thanks A.J. Delgado and G. Gahm for
fruitful discussions. This work was initiated as one of the student
projects during the Nordic-Baltic Optical/NIR and Radio Astronomy Summer
School held in the Tuorla Observatory, Turku, Finland on 8-18th June
2009, where the financial support from NordForsk is greatly
acknowledged. We have made extensive use of SAOImage DS9, developed by
Smithsonian Astrophysical Observatory. This work made use of EURO-VO
software TOPCAT, which is funded by the European Commission through
contracts RI031675 (DCA) and 011892 (VO-TECH) under the 6th Framework
Programme and contracts 212104 (AIDA) and 261541 (VO-ICE) under the 7th
Framework Programme. T.L. acknowledges the support of the Estonian
Ministry for Education and Science, as well as European Social Fund's
Doctoral Studies and Internationalisation Programme DoRa and Kristjan
Jaak Scholarship, which are carried out by Foundation Archimedes. This
work is partly based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA.
NR 54
TC 0
Z9 0
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A75
DI 10.1051/0004-6361/201526532
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800086
ER
PT J
AU Guillemot, L
Smith, DA
Laffon, H
Janssen, GH
Cognard, I
Theureau, G
Desvignes, G
Ferrara, EC
Ray, PS
AF Guillemot, L.
Smith, D. A.
Laffon, H.
Janssen, G. H.
Cognard, I.
Theureau, G.
Desvignes, G.
Ferrara, E. C.
Ray, P. S.
TI The gamma-ray millisecond pulsar deathline, revisited New velocity and
distance measurements
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gamma rays: stars; pulsars: general; parallaxes
ID LARGE-AREA TELESCOPE; RADIO TELESCOPE; NEUTRON-STAR; EMISSION; CATALOG;
PULSATIONS; EVOLUTION; DISCOVERY
AB Context. Millisecond pulsars (MSPs) represent nearly half of the more than 160 currently known gamma-ray pulsars detected by the Large Area Telescope on the Fermi satellite, and a third of all known MSPs are seen in gamma rays. The least energetic gamma-ray MSPs enable us to probe the so-called deathline for high-energy emission, i.e., the spin-down luminosity limit under which pulsars (PSRs) cease to produce detectable high-energy radiation. Characterizing the MSP luminosity distribution helps to determine their contribution to the Galactic diffuse gamma-ray emission.
Aims. Because of the Shklovskii effect, precise proper motion and distance measurements are key ingredients for determining the spin-down luminosities of MSPs accurately. Our aim is to obtain new measurements of these parameters for gamma-ray MSPs when possible, and clarify the relationship between the gamma-ray luminosity of pulsars and their spin-down luminosity. Detecting low spin-down luminosity pulsars in gamma rays and characterizing their spin properties is also particularly interesting for constraining the deathline for high-energy emission.
Methods. We made use of the high-quality pulsar timing data recorded at the Nancay Radio Telescope over several years to characterize the properties of a selection of MSPs. For one of the pulsars, the dataset was complemented with Westerbork Synthesis Radio Telescope observations. The rotation ephemerides derived from this analysis were also used to search the LAT data for new gamma-ray MSPs.
Results. For the MSPs considered in this study, we obtained new transverse proper motion measurements or updated the existing ones, and placed new distance constraints for some of them, with four new timing parallax measurements. We discovered significant GeV gamma-ray signals from four MSPs, i.e., PSRs J0740+6620, J0931-1902, J1455-3330, and J1730-2304. The latter is now the least energetic gamma-ray pulsar found to date. Despite the improved (E) over dot and L gamma estimates, the relationship between these two quantities remains unclear, especially at low (E) over dot values.
C1 [Guillemot, L.; Cognard, I.; Theureau, G.] Univ Orleans, Lab Phys & Chim Environm & Espace, CNRS, F-45071 Orleans 02, France.
[Guillemot, L.; Cognard, I.; Theureau, G.] CNRS INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France.
[Smith, D. A.; Laffon, H.] Univ Bordeaux 1, IN2P3 CNRS, Ctr Etud Nucl Bordeaux Gradignan, BP 120, F-33175 Gradignan, France.
[Janssen, G. H.] Netherlands Inst Radio Astron, ASTRON, Postbus 2 AA, NL-7990 Dwingeloo, Netherlands.
[Desvignes, G.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Ferrara, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ray, P. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
RP Guillemot, L (reprint author), Univ Orleans, Lab Phys & Chim Environm & Espace, CNRS, F-45071 Orleans 02, France.; Guillemot, L (reprint author), CNRS INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France.; Smith, DA; Laffon, H (reprint author), Univ Bordeaux 1, IN2P3 CNRS, Ctr Etud Nucl Bordeaux Gradignan, BP 120, F-33175 Gradignan, France.
EM lucas.guillemot@cnrs-orleans.fr; smith@cenbg.in2p3.fr;
laffon@cenbg.in2p3.fr
OI Ray, Paul/0000-0002-5297-5278
FU Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes
Spatiales in France; Netherlands Foundation for Scientific Research
(NWO)
FX We thank Cees Bassa for helpful discussions and constructive
suggestions. The Fermi-LAT Collaboration acknowledges generous ongoing
support from a number of agencies and institutes that have supported
both the development and the operation of the LAT as well as scientific
data analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council and the Swedish National Space Board in Sweden.
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France. The Nancay
Radio Observatory is operated by the Paris Observatory, associated with
the French Centre National de la Recherche Scientifique (CNRS). The
Westerbork Synthesis Radio Telescope is operated by the Netherlands
Institute for Radio Astronomy (ASTRON) with support from The Netherlands
Foundation for Scientific Research (NWO).
NR 50
TC 3
Z9 3
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A109
DI 10.1051/0004-6361/201527847
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800120
ER
PT J
AU Lindberg, JE
Aalto, S
Muller, S
Marti-Vidal, I
Falstad, N
Costagliola, F
Henkel, C
van der Werf, P
Garcia-Burillo, S
Gonzalez-Alfonso, E
AF Lindberg, J. E.
Aalto, S.
Muller, S.
Marti-Vidal, I.
Falstad, N.
Costagliola, F.
Henkel, C.
van der Werf, P.
Garcia-Burillo, S.
Gonzalez-Alfonso, E.
TI Evidence for a chemically differentiated outflow in Mrk 231
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: individual: Mrk 231; galaxies: active; galaxies: evolution;
quasars: general; ISM: jets and outflows; ISM: molecules
ID VIBRATIONALLY EXCITED HCN; DENSE MOLECULAR GAS; GALAXY MARKARIAN 231;
RELATIVISTIC JETS; STARBURST GALAXY; CO OBSERVATIONS; DRIVEN OUTFLOW;
STAR-FORMATION; HERSCHEL-PACS; FEEDBACK
AB Aims. Our goal is to study the chemical composition of the outflows of active galactic nuclei and starburst galaxies.
Methods. We obtained high-resolution interferometric observations of HCN and HCO+ J = 1 -> 0 and J = 2 -> 1 of the ultraluminous infrared galaxy Mrk 231 with the IRAM Plateau de Bure Interferometer. We also use previously published observations of HCN and HCO+ J = 1 -> 0 and J = 3 -> 2, and HNC J = 1 -> 0 in the same source.
Results. In the line wings of the HCN, HCO+, and HNC emission, we find that these three molecular species exhibit features at distinct velocities which differ between the species. The features are not consistent with emission lines of other molecular species. Through radiative transfer modelling of the HCN and HCO+ outflow emission we find an average abundance ratio X(HCN) = X(HCO+) greater than or similar to 1000. Assuming a clumpy outflow, modelling of the HCN and HCO+ emission produces strongly inconsistent outflow masses.
Conclusions. Both the anti-correlated outflow features of HCN and HCO+ and the different outflow masses calculated from the radiative transfer models of the HCN and HCO+ emission suggest that the outflow is chemically differentiated. The separation between HCN and HCO+ could be an indicator of shock fronts present in the outflow, since the HCN/HCO+ ratio is expected to be elevated in shocked regions. Our result shows that studies of the chemistry in large-scale galactic outflows can be used to better understand the physical properties of these outflows and their effects on the interstellar medium in the galaxy.
C1 [Lindberg, J. E.; Aalto, S.; Muller, S.; Marti-Vidal, I.; Falstad, N.; Costagliola, F.] Chalmers, Dept Earth & Space Sci, Onsala Observ, S-43994 Onsala, Sweden.
[Lindberg, J. E.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Mail Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Costagliola, F.] CNR, Italian ALMA Reg Ctr, Osservatorio Radioastron ORA INAF, Via Gobetti 101, I-40129 Bologna, Italy.
[Henkel, C.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Henkel, C.] King Abdulaziz Univ, Dept Astron, POB 80203, Jeddah 21589, Saudi Arabia.
[van der Werf, P.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Garcia-Burillo, S.] Observ Madrid, Observ Astron Nacl OAN IGN, Alfonso 12,3, Madrid 28014, Spain.
[Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis, Campus Univ, Madrid 28871, Spain.
RP Lindberg, JE (reprint author), Chalmers, Dept Earth & Space Sci, Onsala Observ, S-43994 Onsala, Sweden.; Lindberg, JE (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Mail Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM johan.lindberg@nasa.gov
RI Marti-Vidal, Ivan/A-8799-2017;
OI Marti-Vidal, Ivan/0000-0003-3708-9611; Lindberg,
Johan/0000-0003-3811-4591; Garcia-Burillo, Santiago/0000-0003-0444-6897;
/0000-0002-9931-1313
FU Swedish National Science Council
FX We thank the IRAM PdBI staff for excellent support. This research was
supported by J.E.L.'s appointment to the NASA Postdoctoral Program at
the NASA Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. S.A. thanks the
Swedish National Science Council for grant support. We also thank the
referee Chiara Feruglio for comments and suggestions which significantly
contributed to improving the quality of the manuscript.
NR 44
TC 3
Z9 3
U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A15
DI 10.1051/0004-6361/201527457
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800026
ER
PT J
AU Milligan, RO
Chamberlin, PC
AF Milligan, Ryan O.
Chamberlin, Phillip C.
TI Anomalous temporal behaviour of broadband Ly alpha observations during
solar flares from SDO/EVE
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: activity; Sun: chromosphere; Sun: flares; Sun: UV radiation
ID II SOLSTICE-II; EXTREME-ULTRAVIOLET; EMISSION; MODEL
AB Although it is the most prominent emission line in the solar spectrum, there has been a notable lack of studies devoted to variations in Ly alpha emission during solar flares in recent years. However, the few examples that do exist have shown Ly alpha emission to he a substantial radiator of the total energy budget of solar flares (of the order of 10%). It is also a known driver of fluctuations in the Earth's ionosphere. The EUV Variability Experiment (EVE) on hoard the Solar Dynamics Observatory now provides broadband, photometric Ly alpha data at 10 s cadence with its Multiple EUV Grating Spectrograph-Photometer (MEGS-P) component, and has observed scores of solar flares in the 5 years since it was launched. However, the MEGS-P time profiles appear to display a rise time of tens of minutes around the time of the flare onset. This is in stark contrast to the rapid, impulsive increase observed in other intrinsically chromospheric features (H alpha, Ly beta, LyC, C III, etc.). Furthermore, the emission detected by MEGS-P peaks around the time of the peak of thermal soft X-ray emission and not during the impulsive phase when energy deposition in the chromosphere (often assumed to be in the form of non-thermal electrons) is greatest. The time derivative of Ly alpha lightcurves also appears to resemble that of the time derivative of soft X-rays, reminiscent of the Neupert effect. Given that spectrally-resolved Ly alpha observations during flares from SORCE/SOLSTICE peak during the impulsive phase as expected, this suggests that the atypical behaviour of MEGS-P data is a manifestation of the broadband nature of the observations. This could imply that other lines and/or continuum emission that becomes enhanced during flares could be contributing to the passband. Users are hereby urged to exercise caution when interpreting broadband Ly alpha observations of solar flares. Comparisons have also been made with other broadband Ly alpha photometers such as PROBA2/LYRA and GOES/EUVS-E.
C1 [Milligan, Ryan O.] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland.
[Milligan, Ryan O.; Chamberlin, Phillip C.] NASA, Solar Phys Lab, Heliophys Sci Div, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
[Milligan, Ryan O.] Catholic Univ Amer, Dept Phys, 620 Michigan Ave Northeast, Washington, DC 20064 USA.
RP Milligan, RO (reprint author), Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland.; Milligan, RO (reprint author), NASA, Solar Phys Lab, Heliophys Sci Div, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.; Milligan, RO (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave Northeast, Washington, DC 20064 USA.
EM r.milligan@qub.ac.uk
RI Chamberlin, Phillip/C-9531-2012
OI Chamberlin, Phillip/0000-0003-4372-7405
FU NASA LWS/TRT grant [NNX11AQ53G]; LWS/SDO Data Analysis grant
[NNX14AE070G]
FX The authors would like to thank the anonymous referee for the
constnictive comments that greatly enhanced this paper. They also thank
Marty Snow (LASP) for access to the high-cadence SOLSTICE data, Janet
Machol (NOAA) for help with the GOES EUVS-E data, and Mihalis
Mathioudakis (QUB) for many stimulating discussions on this issue. This
work was supported by NASA LWS/TR&T grant NNX11AQ53G and LWS/SDO Data
Analysis grant NNX14AE070G.
NR 25
TC 1
Z9 1
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A123
DI 10.1051/0004-6361/201526682
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800134
ER
PT J
AU Pon, A
Johnstone, D
Caselli, P
Fontani, F
Palau, A
Butler, MJ
Kaufman, M
Jimenez-Serra, I
Tan, JC
AF Pon, A.
Johnstone, D.
Caselli, P.
Fontani, F.
Palau, A.
Butler, M. J.
Kaufman, M.
Jimenez-Serra, I.
Tan, J. C.
TI Mid-J CO shock tracing observations of infrared dark clouds II. Low-J CO
constraints on excitation, depletion, and kinematics
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: clouds; stars: formation; ISM: molecules; ISM: kinematics and
dynamics; ISM: structure; ISM: abundances
ID MASSIVE-STAR-FORMATION; LOW-VELOCITY SHOCKS; PRE-STELLAR CORES;
MOLECULAR CLOUDS; GALACTIC PLANE; SUBMILLIMETER EMISSION;
INTERSTELLAR-MEDIUM; INITIAL CONDITIONS; COLOGNE DATABASE; FORMATION
RATES
AB Infrared dark clouds are kinematically complex molecular structures in the interstellar medium that can host sites of massive star formation. We present maps measuring 4 square arcminutes of the (CO)-C-12, (CO)-C-13, and (CO)-O-18 J = 3 to 2 lines from selected locations within the C and F (G028.37 + 00.07 and G034.43 + 00.24) infrared dark clouds (IRDCs), as well as single pointing observations of the (CO)-C-13 and (CO)-O-18 J = 2 to 1 lines towards three cores within these clouds. We derive CO gas temperatures throughout the maps and find that CO is significantly frozen out within these IRDCs. We find that the CO depletion tends to be the highest near column density peaks with maximum depletion factors between 5 and 9 in IRDC F and between 16 and 31 in IRDC C. We also detect multiple velocity components and complex kinematic structure in both IRDCs. Therefore, the kinematics of IRDCs seem to point to dynamically evolving structures yielding dense cores with considerable depletion factors.
C1 [Pon, A.; Caselli, P.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Pon, A.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Johnstone, D.] Joint Astron Ctr, 660 North Aohoku Pl,Univ Pk, Hilo, HI 96720 USA.
[Johnstone, D.] NRC Herzberg Inst Astrophys, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada.
[Johnstone, D.] Univ Victoria, Dept Phys & Astron, POB 3055 STN CSC, Victoria, BC V8W 3P6, Canada.
[Fontani, F.] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy.
[Palau, A.] Univ Nacl Autonoma Mexico, Inst Radioastron & Astrofis, POB 3-72, Morelia 58090, Michoacan, Mexico.
[Butler, M. J.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Kaufman, M.] San Jose State Univ, Dept Phys & Astron, One Washington Sq, San Jose, CA 95192 USA.
[Kaufman, M.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA.
[Jimenez-Serra, I.] UCL, Dept Phys & Astron, 132 Hampstead Rd, London NW1 2PS, England.
[Tan, J. C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Tan, J. C.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA.
RP Pon, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.; Pon, A (reprint author), Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
EM apon@uwo.ca
FU European Research Council (ERC) [320620]; Natural Sciences and
Engineering Research Council (NSERC) Discovery Grant; UNAM-DGAPA-PAPIIT
grant, Mexico [IA102815]; STFC [ST/L004801/1]
FX We would like to thank our anonymous referee for helping improve the
clarity and quality of this paper. The authors would like to thank Dr.
N. Bailey, Dr. J. Bailey, Dr. S. Sadavoy, Dr. J. D. Henshaw, and A.
Barnes for many insightful conversations regarding the data presented in
this paper. The authors would also like to thank the Joint Astronomy
Center for their assistance in reducing the JCMT data. Andy Pon and P.C.
acknowledge the financial support of the European Research Council (ERC;
project PALs 320620). D. J. acknowledges support from a Natural Sciences
and Engineering Research Council (NSERC) Discovery Grant. Aina Palau
acknowledges financial support from UNAM-DGAPA-PAPIIT IA102815 grant,
Mexico. I.J.-S. acknowledges the financial support received from the
STFC through an Ernest Rutherford Fellowship (proposal number
ST/L004801/1). This research has made use of the Smithsonian
Astrophysical Observatory (SAO)/National Aeronautics and Space
Administration's (NASA's) Astrophysics Data System (ADS). This research
has made use of the astro-ph archive. Some spectral line data were taken
from the Spectral Line Atlas of Interstellar Molecules (SLAIM)
(Available at http://www.splatalogue.net). (F. J. Lovas, priv. comm.;
Remijan et al. 2007). More information regarding the GILDAS CLASS
software can be found at http://www.iram.fr/IRAMFR/GILDAS. The James
Clerk Maxwell Telescope has historically been operated by the Joint
Astronomy Centre on behalf of the Science and Technology Facilities
Council of the United Kingdom, the National Research Council of Canada
and the Netherlands Organisation for Scientific Research.
NR 76
TC 4
Z9 4
U1 2
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A96
DI 10.1051/0004-6361/201527154
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800107
ER
PT J
AU Rauch, T
Quinet, P
Hoyer, D
Werner, K
Demleitner, M
Kruk, JW
AF Rauch, T.
Quinet, P.
Hoyer, D.
Werner, K.
Demleitner, M.
Kruk, J. W.
TI Stellar laboratories VI. New Mo IV-VII oscillator strengths and the
molybdenum abundance in the hot white dwarfs G191-B2B and RE 0503-289
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE atomic data; line: identification; stars: abundances; stars: individual:
G191-B2B; stars: individual: RE0503-289; virtual observatory tools
ID CONSISTENT DIFFUSION-MODELS; ELEMENTAL COMPOSITION; SPECTRAL-ANALYSIS;
ATOMIC-DATA; IRON-GROUP; SEQUENCE; IONS; ATMOSPHERES; ULTRAVIOLET;
VALIDATION
AB Context. For the spectral analysis of high-resolution and high signal-to-noise (S/N) spectra of hot stars, state-of-the-art non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that is used for their calculation.
Aims. To identify molybdenum lines in the ultraviolet (UV) spectra of the DA-type white dwarf G191-B2B and the DO-type white dwarf RE 0503-289 and, to determine their photospheric Mo abundances, reliable Mo IV-VII oscillator strengths are used.
Methods. We newly calculated Mo IV-VII oscillator strengths to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models for the analysis of Mo lines exhibited in high-resolution and high S/N UV observations of RE 0503-289.
Results. We identified 12 Mo V and 9 Mo VI lines in the UV spectrum of RE 0503-289 and measured a photospheric Mo abundance of 1.2-3.0 x 10(-4) (mass fraction, 22 500-56 400 times the solar abundance). In addition, from the As v and Sn IV resonance lines, we measured mass fractions of arsenic (0.5-1.3 x 10(-5), about 300-1200 times solar) and tin (1.3-3.2 x 10(-4), about 14 300-35 200 times solar). For G191-B2B, upper limits were determined for the abundances of Mo (5.3 x 10(-7), 100 times solar) and, in addition, for Kr (1.1 x 10(-6), 10 times solar) and Xe (1.7 x 10(-7), 10 times solar). The arsenic abundance was determined (2.3-5.9 x 10(-7), about 21-53 times solar). A new, registered German Astrophysical Virtual Observatory (GAVO) service, TOSS, has been constructed to provide weighted oscillator strengths and transition probabilities.
Conclusions. Reliable measurements and calculations of atomic data are a prerequisite for stellar-atmosphere modeling. Observed Mo V-VI line profiles in the UV spectrum of the white dwarf RE 0503-289 were well reproduced with our newly calculated oscillator strengths. For the first time, this allowed the photospheric Mo abundance in a white dwarf to be determined.
C1 [Rauch, T.; Hoyer, D.; Werner, K.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
[Quinet, P.] Univ Mons UMONS, Phys Atom & Astrophys, B-7000 Mons, Belgium.
[Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium.
[Demleitner, M.] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany.
[Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rauch, T (reprint author), Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
EM rauch@astro.uni-tuebingen.de
FU German Aerospace Center (DLR) [05 OR 1402, 50 OR 1501]; Federal Ministry
of Education and Research (BMBF) at Tubingen [05 AC 6 VTB, 05 AC 11
VTB]; Federal Ministry of Education and Research (BMBF) at Heidelberg
[05 AC 11 VH3]; Belgian FRS-FNRS; NASA [NAS5-26555]; NASA Office of
Space Science [NNX09AF08G]
FX T.R. and D H. are supported by the German Aerospace Center (DLR, grants
05 OR 1402 and 50 OR 1501, respectively). The GAVO project had been
supported by the Federal Ministry of Education and Research (BMBF) at
Tubingen (05 AC 6 VTB, 05 AC 11 VTB) and is funded at Heidelberg (05 AC
11 VH3). Financial support from the Belgian FRS-FNRS is also
acknowledged. P.Q. is research director of this organization. We thank
our referee, Stephane Vennes, for constructive criticism. Some of the
data presented in this paper were obtained from the Mikulski Archive for
Space Telescopes (MAST). STScI is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555. Support for MAST for non-HST data is provided by the NASA
Office of Space Science via grant NNX09AF08G and by other grants and
contracts. This research has made use of NASA's Astrophysics Data System
and the SIMBAD database, operated at CDS, Strasbourg, France. The TOSS
service (http://dc.g-vo.org/TOSS) that provides weighted oscillator
strengths and transition probabilities was constructed as part of the
activities of the German Astrophysical Virtual Observatory.
NR 47
TC 2
Z9 2
U1 1
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A39
DI 10.1051/0004-6361/201527324
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800050
ER
PT J
AU van Kempen, TA
Hogerheijde, MR
van Dishoeck, EF
Kristensen, LE
Belloche, A
Klaassen, PD
Leurini, S
San Jose-Garcia, I
Aykutalp, A
Choi, Y
Endo, A
Frieswijk, W
Harsono, D
Karska, A
Koumpia, E
van der Marel, N
Nagy, Z
Perez-Beaupuits, JP
Risacher, C
van Weeren, RJ
Wyrowski, F
Yildiz, UA
Gusten, R
Boland, W
Baryshev, A
AF van Kempen, T. A.
Hogerheijde, M. R.
van Dishoeck, E. F.
Kristensen, L. E.
Belloche, A.
Klaassen, P. D.
Leurini, S.
San Jose-Garcia, I.
Aykutalp, A.
Choi, Y.
Endo, A.
Frieswijk, W.
Harsono, D.
Karska, A.
Koumpia, E.
van der Marel, N.
Nagy, Z.
Perez-Beaupuits, J. -P.
Risacher, C.
van Weeren, R. J.
Wyrowski, F.
Yildiz, U. A.
Guesten, R.
Boland, W.
Baryshev, A.
TI Outflow forces in intermediate-mass star formation
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE circumstellar matter; stars: formation; ISM: jets and outflows;
submillimeter: ISM
ID YOUNG STELLAR OBJECTS; HIGH-J CO; HERSCHEL-PACS SPECTROSCOPY; PROTOSTAR
SERPENS SMM1; VELA MOLECULAR CLOUDS; JCMT LEGACY SURVEY; NGC-7129 FIRS
2; FORMING REGIONS; ENVELOPE STRUCTURE; CLASS-0 SOURCES
AB Context. Protostars of intermediate-mass provide a bridge between theories of low-and high-mass star formation. Molecular outflows emerging from such sources can be used to determine the influence of fragmentation and multiplicity on protostellar evolution through the apparent correlation of outflow forces of intermediate-mass protostars with the total luminosity instead of the individual luminosity.
Aims. The aim of this paper is to derive outflow forces from outflows of six intermediate-mass protostellar regions and validate the apparent correlation between total luminosity and outflow force seen in earlier work, as well as remove uncertainties caused by different methodologies.
Methods. By comparing CO 6-5 observations obtained with APEX with non-LTE radiative transfer model predictions, the optical depths, temperatures and densities of the gas of the molecular outflows are derived. Outflow forces, dynamical timescales, and kinetic luminosities are subsequently calculated.
Results. Outflow parameters, including the forces, were derived for all sources. Temperatures in excess of 50 K were found for all flows, in line with recent low-mass results. However, comparison with other studies could not corroborate conclusions from earlier work on intermediate-mass protostars which hypothesized that fragmentation enhances outflow forces in clustered intermediate-mass star formation. Any enhancement in comparison with the classical relation between outflow force and luminosity can be attributed to the use of a higher excitation line and improvement in methods. They are in line with results from low-mass protostars using similar techniques.
Conclusions. The role of fragmentation on outflows is an important ingredient to understand clustered star formation and the link between low- and high-mass star formation. However, detailed information on spatial scales of a few 100 AU, covering all individual members is needed to make the necessary progress.
C1 [van Kempen, T. A.; Hogerheijde, M. R.; van Dishoeck, E. F.; Kristensen, L. E.; Klaassen, P. D.; San Jose-Garcia, I.; Harsono, D.; Karska, A.; van der Marel, N.; van Weeren, R. J.; Yildiz, U. A.; Boland, W.] Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
[van Kempen, T. A.] Joint ALMA Off, Ave Alonso Cordova 3107, Santiago, Chile.
[van Dishoeck, E. F.; Karska, A.] Max Planck Inst Extraterr Phys, Giessenbachstr 2, D-85478 Garching, Germany.
[Kristensen, L. E.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Belloche, A.; Leurini, S.; Perez-Beaupuits, J. -P.; Risacher, C.; Wyrowski, F.; Guesten, R.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Klaassen, P. D.] Royal Observ, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Aykutalp, A.; Choi, Y.; Koumpia, E.; Nagy, Z.; Baryshev, A.] Univ Groningen, Kapteyn Inst, Landleven 12, NL-9747 AD Groningen, Netherlands.
[Aykutalp, A.] Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy.
[Choi, Y.; Koumpia, E.; Nagy, Z.; Risacher, C.; Baryshev, A.] SRON Netherlands Inst Space Res, Low Energy Astrophys Div, Postbus 800, NL-9700 AV Groningen, Netherlands.
[Endo, A.] Delft Univ Technol, Fac Elect Engn Math & Comp Sci, Dept Microelect, NL-2628 CD Delft, Netherlands.
[Endo, A.] Delft Univ Technol, Kavli Inst Nanosci, Dept Quantum Nanosci, Lorentzweg 1, NL-2628 CJ Delft, Netherlands.
[Frieswijk, W.] Netherlands Inst Radio Astron ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Karska, A.] Adam Mickiewicz Univ, Fac Phys, Astron Observ Inst, Sloneczna 36, PL-60286 Poznan, Poland.
[Yildiz, U. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Boland, W.] Netherlands Res Sch Astron, POB 9513, NL-2300 RA Leiden, Netherlands.
RP van Kempen, TA (reprint author), Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.; van Kempen, TA (reprint author), Joint ALMA Off, Ave Alonso Cordova 3107, Santiago, Chile.
EM kempen@strw.leidenuniv.nl
RI Kristensen, Lars/F-4774-2011; Yildiz, Umut/C-5257-2011; Karska,
Agata/O-5311-2016;
OI Kristensen, Lars/0000-0003-1159-3721; Yildiz, Umut/0000-0001-6197-2864;
Karska, Agata/0000-0001-8913-925X; Perez-Beaupuits,
Juan-Pablo/0000-0003-3536-2274; van Weeren, Reinout/0000-0002-0587-1660
FU Allegro ARC node in Leiden; NOVA (Nederlandse Onderzoeksschool voor
Astronomie); NWO (Nederlandse Organisatie voor Wetenschappelijk
Onderzoek); NASA through the Einstein Postdoctoral grant - Chandra X-ray
Center [PF2-130104]; NASA [NAS8-03060]; Polish National Science Center
grant [2013/11/N/ST9/00400]; Foundation for Polish Science (FNP);
Netherlands Organization for Scientific Research (NWO) [600.063.310.10]
FX T.v.K. is supported by the Allegro ARC node in Leiden and NOVA
(Nederlandse Onderzoeksschool voor Astronomie) and NWO (Nederlandse
Organisatie voor Wetenschappelijk Onderzoek). R.J.v.W. acknowledges
support provided by NASA through the Einstein Postdoctoral grant number
PF2-130104 awarded by the Chandra X-ray Center, which is operated by the
Smithsonian Astrophysical Observatory for NASA under contract
NAS8-03060. A.K. acknowledges support from the Polish National Science
Center grant 2013/11/N/ST9/00400 and the Foundation for Polish Science
(FNP). Construction of CHAMP+ was a collaboration between the
Max-Planck-Institut fur Radioastronomie Bonn, Germany; SRON Netherlands
Institute for Space Research, Groningen, The Netherlands; The
Netherlands Research School for Astronomy (NOVA); and the Kavli
Institute of Nanoscience at Delft University of Technology, the
Netherlands; with support from the Netherlands Organization for
Scientific Research (NWO) grant 600.063.310.10. We thank the APEX staff,
in particular the scientists (Per Bergman, Andreas Lundgren, Michael
Dumke, Francisco Montenegro and Rodrigo Parra) and operators (Francisco
"Pancho" Azagra, Claudio Agurto, Felipe Mac Auliffe, Paulina Venegas and
Mauricio Martinez) for their warm welcome over the years.
NR 67
TC 2
Z9 2
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A17
DI 10.1051/0004-6361/201424725
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800028
ER
PT J
AU Wedlund, CS
Kallio, E
Alho, M
Nilsson, H
Wieser, GS
Gunell, H
Behar, E
Pusa, J
Gronoff, G
AF Wedlund, C. Simon
Kallio, E.
Alho, M.
Nilsson, H.
Wieser, G. Stenberg
Gunell, H.
Behar, E.
Pusa, J.
Gronoff, G.
TI The atmosphere of comet 67P/Churyumov-Gerasimenko diagnosed by
charge-exchanged solar wind alpha particles
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE comets: general; comets: individual: 67P/Churyumov-Gerasimenko;
instrumentation: detectors; solar wind; methods: analytical
ID ROSETTA PLASMA CONSORTIUM; INTEGRAL CROSS-SECTIONS; ELECTRON-CAPTURE;
5-KEV PROTONS; IONS; ENVIRONMENT; GASES; COLLISIONS; EVOLUTION; MISSION
AB Context. The ESA/Rosetta mission has been orbiting comet 67P/Churyumov-Gerasimenko since August 2014, measuring its dayside plasma environment, The ion spectrometer onboard Rosetta has detected two ion populations, one energetic with a solar wind origin (H+, He2+, He+), the other at lower energies with a cometary origin (water group ions such as H2O+). He+ ions arise mainly from charge-exchange between solar wind alpha particles and cometary neutrals such as H2O.
Aims. The He+ and He2+ ion fluxes measured by the Rosetta Plasma Consortium Ion Composition Analyser (RPC-ICA) give insight into the composition of the dayside neutral coma, into the importance of charge-exchange processes between the solar wind and cometary neutrals, and into the way these evolve when the comet draws closer to the Sun.
Methods. We combine observations by the ion spectrometer RPC-ICA onboard Rosetta with calculations from an analytical model based on a collisionless neutral Haser atmosphere and nearly undisturbed solar wind conditions.
Results. Equivalent neutral outgassing rates Q can be derived using the observed RPC-ICA He+/He2+ particle flux ratios as input into the analytical model in inverse mode. A revised dependence of Q on heliocentric distance R-h in AU is found to R-h(-7.06) between 1.8 and 3.3 AU, suggesting that the activity in 2015 differed from that of the 2008 perihelion passage. Conversely, using an outgassing rate determined from optical remote sensing measurements from Earth, the forward analytical model results are in relatively good agreement with the measured RPC-ICA flux ratios, Modelled ratios in a 2D spherically-symmetric plane are also presented, shoyving that charge exchange is most efficient with solar wind protons. Detailed cometocentric profiles of these ratios are also presented.
Conclusions. In conclusion, we show that, with the help of a simple analytical model of charge-exchange processes, a mass-capable ion spectrometer such as RPC-ICA can be used as a "remote-sensing" instrument for the neutral cometary atmosphere.
C1 [Wedlund, C. Simon; Kallio, E.; Alho, M.; Pusa, J.] Aalto Univ, Sch Elect Engn, Dept Radio Sci & Engn, POB 13000, Aalto 00076, Finland.
[Wedlund, C. Simon] Univ Oslo, Dept Phys, Box 1048 Blindern, N-0316 Oslo, Norway.
[Nilsson, H.; Wieser, G. Stenberg; Behar, E.] Swedish Inst Space Phys, Box 812, S-98128 Kiruna, Sweden.
[Nilsson, H.; Behar, E.] Lulea Univ Technol, Dept Comp Sci Elect & Space Engn, Rymdcampus 1, S-98128 Kiruna, Sweden.
[Gunell, H.] Belgian Inst Space Aeron, Ave Circulaire 3, B-1180 Brussels, Belgium.
[Gronoff, G.] NASA, Langley Res Ctr, Sci Directorate, Chem & Dynam Branch, Hampton, VA 23665 USA.
[Gronoff, G.] SSAI, Hampton, VA USA.
RP Wedlund, CS (reprint author), Aalto Univ, Sch Elect Engn, Dept Radio Sci & Engn, POB 13000, Aalto 00076, Finland.; Wedlund, CS (reprint author), Univ Oslo, Dept Phys, Box 1048 Blindern, N-0316 Oslo, Norway.
EM cyril.simon.wedlund@gmail.com
RI Kallio, Esa/F-9410-2014;
OI Kallio, Esa/0000-0002-9791-804X; Gronoff, Guillaume/0000-0002-0331-7076
FU Academy of Finland; Research Council of Norway [240000]; Swedish
National Space Board [108/12, 112/13]; Belgian Science Policy Office
through the Solar-Terrestrial Centre of Excellence;
PRODEX/ROSETTA/ROSINA PEA [4000107705]; CNRS; CNES; Observatoire de
Paris; Universite Paul Sabatier, Toulouse; NASA Astrobiology Institute
Grant [NNX15AE05G]; NASA HIDEE program Grant [NNH15CO73C]
FX Rosetta is a European Space Agency (ESA) mission with contributions from
its member states and the National Aeronautics and Space Administration
(NASA). This study was supported by the Academy of Finland and, in part,
by the Research Council of Norway grant No. 240000. The work on RPC-ICA
was funded by the Swedish National Space Board under contracts 108/12
and 112/13. Work at the Belgian Institute for Space Aeronomy was
supported by the Belgian Science Policy Office through the
Solar-Terrestrial Centre of Excellence and by PRODEX/ROSETTA/ROSINA PEA
4000107705. First selection of events in this study was performed with
the AMDA science analysis system provided by the Centre de Donnees de la
Physique des Plasmas (CDPP) supported by CNRS, CNES, Observatoire de
Paris and Universite Paul Sabatier, Toulouse. G.G. is supported by the
NASA Astrobiology Institute Grant NNX15AE05G and by the NASA HIDEE
program Grant NNH15CO73C. C.S.W. thanks T.E. Cravens (University of
Kansas, USA), W.J. Miloch (University of Oslo, Norway) and, last but not
least, M. Simon Wedlund for useful discussions.
NR 44
TC 4
Z9 4
U1 2
U2 5
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2016
VL 587
AR A154
DI 10.1051/0004-6361/201527532
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DF8EK
UT WOS:000371589800165
ER
PT J
AU Hamill, P
Iraci, LT
Yates, EL
Gore, W
Bui, TP
Tanaka, T
Loewenstein, M
AF Hamill, Patrick
Iraci, Laura T.
Yates, Emma L.
Gore, Warren
Bui, T. Paul
Tanaka, Tomoaki
Loewenstein, Max
TI A New Instrumented Airborne Platform for Atmospheric Research
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID METEOROLOGICAL MEASUREMENT SYSTEM; CALIBRATION; CALIFORNIA; AIRCRAFT;
METHANE; CO2
AB The NASA Ames Research Center operates a new research platform for atmospheric studies: an instrumented Alpha Jet. The present complement of instruments allows for the determination of carbon dioxide, ozone, water vapor, and methane concentrations as well as measurements of three-dimensional wind speeds, temperature, and pressure. Planned future instrumentation includes an Air-Core sampler and an instrument to measure formaldehyde. We give examples of measurements that have been made, including measurements carried out during a downward spiral over an expected methane source. An attractive property of this airborne system is its ability to respond rapidly to unexpected atmospheric events such as large forest fires or severe air quality events.
C1 [Hamill, Patrick; Iraci, Laura T.; Yates, Emma L.; Gore, Warren; Bui, T. Paul; Tanaka, Tomoaki; Loewenstein, Max] NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.
[Hamill, Patrick] San Jose State Univ, San Jose, CA 95192 USA.
RP Hamill, P (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.
EM patrick.hamill@sjsu.edu
FU NASA Ames Research Center; NASA [NNX-13AM21G]
FX The authors acknowledge the ongoing support and partnership of H211,
LLC, with particular thanks to K. Ambrose, R. Simone, and R. Fisher.
Funding for instrumentation and aircraft integration was received from
the NASA Ames Research Center Director's Fund and the NASA Science
Innovation Fund. Technical contributions from Z. Young, E. Quigley, A.
Trias, and R. Vogler were fundamental to the success of AJAX. The COWGAS
project was funded by NASA Grant NNX-13AM21G.
NR 15
TC 1
Z9 1
U1 7
U2 10
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD MAR
PY 2016
VL 97
IS 3
BP 397
EP 404
DI 10.1175/BAMS-D-14-00241.1
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DI9DV
UT WOS:000373802600001
ER
PT J
AU Ruf, CS
Atlas, R
Chang, PS
Clarizia, MP
Garrison, JL
Gleason, S
Katzberg, SJ
Jelenak, Z
Johnson, JT
Majumdar, SJ
O'brien, A
Posselt, DJ
Ridley, AJ
Rose, RJ
Zavorotny, VU
AF Ruf, Christopher S.
Atlas, Robert
Chang, Paul S.
Clarizia, Maria Paola
Garrison, James L.
Gleason, Scott
Katzberg, Stephen J.
Jelenak, Zorana
Johnson, Joel T.
Majumdar, Sharanya J.
O'brien, Andrew
Posselt, Derek J.
Ridley, Aaron J.
Rose, Randall J.
Zavorotny, Valery U.
TI New Ocean Winds Satellite Mission to Probe Hurricanes and Tropical
Convection
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID GPS SIGNALS; SCATTEROMETER; SCATTERING; GNSS
AB The Cyclone Global Navigation Satellite System (CYGNSS) is a new NASA earth science mission scheduled to be launched in 2016 that focuses on tropical cyclones (TCs) and tropical convection. The mission's two primary objectives are the measurement of ocean surface wind speed with sufficient temporal resolution to resolve short-time-scale processes such as the rapid intensification phase of TC development and the ability of the surface measurements to penetrate through the extremely high precipitation rates typically encountered in the TC inner core. The mission's goal is to support significant improvements in our ability to forecast TC track, intensity, and storm surge through better observations and, ultimately, better understanding of inner-core processes. CYGNSS meets its temporal sampling objective by deploying a constellation of eight satellites. Its ability to see through heavy precipitation is enabled by its operation as a bistatic radar using low-frequency GPS signals. The mission will deploy an eight-spacecraft constellation in a low-inclination (35 degrees) circular orbit to maximize coverage and sampling in the tropics. Each CYGNSS spacecraft carries a four-channel radar receiver that measures GPS navigation signals scattered by the ocean surface. The mission will measure inner-core surface winds with high temporal resolution and spatial coverage, under all precipitating conditions, and over the full dynamic range of TC wind speeds.
C1 [Ruf, Christopher S.; Clarizia, Maria Paola; Posselt, Derek J.; Ridley, Aaron J.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Atlas, Robert] NOAA AOML, Miami, FL USA.
[Chang, Paul S.; Jelenak, Zorana] NOAA NESDIS STAR, College Pk, MD USA.
[Garrison, James L.] Purdue Univ, W Lafayette, IN 47907 USA.
[Gleason, Scott; Rose, Randall J.] Southwest Res Inst, Boulder, CO USA.
[Katzberg, Stephen J.] NASA LaRC, Hampton, VA USA.
[Johnson, Joel T.; O'brien, Andrew] Ohio State Univ, Columbus, OH 43210 USA.
[Majumdar, Sharanya J.] Univ Miami, Coral Gables, FL 33124 USA.
[Zavorotny, Valery U.] NOAA ESRL, Boulder, CO USA.
RP Ruf, CS (reprint author), Univ Michigan, Dept Climate & Space, 2455 Hayward St, Ann Arbor, MI 48109 USA.
EM cruf@umich.edu
RI Jelenak, Zorana/F-5596-2010; Chang, Paul/F-5580-2010; Atlas,
Robert/A-5963-2011; Ridley, Aaron/F-3943-2011
OI Jelenak, Zorana/0000-0003-0510-2973; Chang, Paul/0000-0001-5113-0938;
Atlas, Robert/0000-0002-0706-3560; Ridley, Aaron/0000-0001-6933-8534
FU NASA Science Mission Directorate [NNL13AQ00C]
FX The work presented was supported in part by NASA Science Mission
Directorate Contract NNL13AQ00C. The authors would also like to thank
Dave Nolan for providing the nature run simulation data and Brian
McNoldy for producing the spatial sampling image (Fig 7).
NR 29
TC 12
Z9 12
U1 3
U2 14
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD MAR
PY 2016
VL 97
IS 3
DI 10.1175/BAMS-D-14-00218.1
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DI9DQ
UT WOS:000373802100002
ER
EF