FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Thompson, DJ
AF Thompson, D. J.
TI The Gamma-ray Sky with Fermi
SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS
LA English
DT Proceedings Paper
CT 4th International Conference on Particle and Fundamental Physics in
Space
CY NOV 05-07, 2012
CL CERN, Geneva, SWITZERLAND
SP INFN
HO CERN
DE gamma rays; pulsars; active galactic nuclei; gamma-ray burst
ID LARGE-AREA TELESCOPE; BLIND FREQUENCY SEARCHES; MILLISECOND PULSARS;
SPACE-TELESCOPE; DWARF GALAXIES; LAT DISCOVERY; CRAB-NEBULA; LOCAL
GROUP; EMISSION; CLUSTERS
AB Gamma rays reveal extreme, nonthermal conditions in the Universe. The Fermi Gamma-ray Space Telescope has been exploring the gamma-ray sky for more than four years, enabling a search for powerful transients like gamma-ray bursts, solar flares, and flaring active galactic nuclei, as well as long-term studies including pulsars, binary systems, supernova remnants, and searches for predicted sources of gamma rays such as clusters of galaxies. Some results include a stringent limit on Lorentz invariance violation derived from a gamma-ray burst, unexpected gamma-ray variability from the Crab Nebula, a huge gamma-ray structure in the direction of the center of our Galaxy, and strong constraints on some Weakly Interacting Massive Particle (WIMP) models for dark matter.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Thompson, DJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM David.J.Thompson@nasa.gov
NR 45
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0920-5632
EI 1873-3832
J9 NUCL PHYS B-PROC SUP
JI Nucl. Phys. B-Proc. Suppl.
PD OCT-NOV
PY 2013
VL 243
BP 58
EP 63
DI 10.1016/j.nuclphysbps.2013.09.022
PG 6
WC Physics, Particles & Fields
SC Physics
GA 293GI
UT WOS:000329959000008
ER
PT J
AU Gehrels, N
Cannizzo, JK
AF Gehrels, N.
Cannizzo, J. K.
TI NASA's Dark Matter & Dark Energy Programs
SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS
LA English
DT Proceedings Paper
CT 4th International Conference on Particle and Fundamental Physics in
Space
CY NOV 05-07, 2012
CL CERN, Geneva, SWITZERLAND
SP INFN
HO CERN
DE gravitational lensing; techniques: spectroscopic; supernovae: general;
cosmology: cosmic microwave background; cosmological parameters; dark
matter; large-scale structure of universe; theory
ID HUBBLE-SPACE-TELESCOPE; PROBE WMAP OBSERVATIONS; IA SUPERNOVAE; LIGHT
CURVES; ACCELERATING UNIVERSE; CONSTRAINTS; COSMOLOGY; CHANDRA; SAMPLE
AB We present an overview of selected high value scientific results and prospects for future advances from NASA's "Dark" missions, i.e., those covering dark matter (DM) and dark energy (DE). This includes current missions HST, Chandra, Swift, GALEX, Suzaku, Fermi, and future missions JWST and WFIRST. These missions and earlier ones, such as WMAP, have brought about a revolution in our understanding of the fundamental properties of the universe - its age, rate of expansion, deceleration history, and composition (i.e., relative mix of luminous matter, dark matter, and dark energy). The next chapters in this story will be written by JWST and WFIRST. JWST was the highest priority of the 2000 Decadal Survey. It will observe in the near and medium infrared, and revolutionize our understanding of the high redshift universe. WFIRST is the highest ranked large space mission of the 2010 Decadal Survey. It is a NASA observatory designed to perform wide-field imaging and slitless spectroscopic surveys of the NIR sky (0.7 - 2.5 mu) WFIRST will: (i) measure the expansion history of the universe, and thereby constrain dark energy, (ii) find Earth-like planets around other stars using microlensing, and (iii) perform surveys that are similar to 100 times more sensitive than current NIR surveys.
C1 [Gehrels, N.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Div, Greenbelt, MD 20771 USA.
[Cannizzo, J. K.] Univ Maryland Baltimore Cty, CRESST Joint Ctr Astrophys, Baltimore, MD 21250 USA.
RP Gehrels, N (reprint author), NASA, Goddard Space Flight Ctr, Astroparticle Phys Div, Greenbelt, MD 20771 USA.
EM neil.gehrels@nasa.gov
NR 24
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0920-5632
EI 1873-3832
J9 NUCL PHYS B-PROC SUP
JI Nucl. Phys. B-Proc. Suppl.
PD OCT-NOV
PY 2013
VL 243
BP 64
EP 69
DI 10.1016/j.nuclphysbps.2013.09.010
PG 6
WC Physics, Particles & Fields
SC Physics
GA 293GI
UT WOS:000329959000009
ER
PT J
AU Yamamoto, A
Mitchell, JW
AF Yamamoto, Akira
Mitchell, John W.
TI Search for Primary Antiparticles and Cosmological Antimatter with BESS
SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS
LA English
DT Proceedings Paper
CT 4th International Conference on Particle and Fundamental Physics in
Space
CY NOV 05-07, 2012
CL CERN, Geneva, SWITZERLAND
SP INFN
HO CERN
DE Cosmic ray; antiparticle; antimatter; early universe; superconducting
spectrometer; BESS
ID BALLOON-BORNE EXPERIMENT; COSMIC-RAY ANTIPROTONS; MOUNTAIN ALTITUDE;
HELIUM SPECTRA; SOLAR MINIMUM; MUON SPECTRA; SPECTROMETER; ANTIHELIUM;
FLUX; PROTON
AB The Balloon-borne Experiment with a Superconducting Spectrometer (BESS) has performed precise measurements of low-energy cosmic-ray antiproton spectra to investigate signatures of exotic origins such as dark matter candidates or primordial black holes, and has searched for antimatter in cosmic rays that might reach Earth from antimatter domains formed in the early Universe. BESS carried out its second Antarctic flight, BESS-Polar II, during the 2007-2008 Austral Summer, and obtained over 4.7 billion cosmic-ray events from 24.5 days of observation during a solar-minimum period, when the sensitivity of the low-energy antiproton measurements to a possible primary source would be greatest. Here, we report the scientific results.
C1 [Yamamoto, Akira] High Energy Accelerator Res Org, KEK, Tsukuba, Ibaraki, Japan.
[Mitchell, John W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Yamamoto, A (reprint author), High Energy Accelerator Res Org, KEK, Tsukuba, Ibaraki, Japan.
EM akira.yamamoto@kek.jp
NR 49
TC 1
Z9 1
U1 0
U2 3
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0920-5632
EI 1873-3832
J9 NUCL PHYS B-PROC SUP
JI Nucl. Phys. B-Proc. Suppl.
PD OCT-NOV
PY 2013
VL 243
BP 92
EP 97
DI 10.1016/j.nuclphysbps.2013.09.027
PG 6
WC Physics, Particles & Fields
SC Physics
GA 293GI
UT WOS:000329959000013
ER
PT J
AU Turyshev, SG
AF Turyshev, Slava G.
TI Testing Fundamental Gravitation in Space
SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS
LA English
DT Proceedings Paper
CT 4th International Conference on Particle and Fundamental Physics in
Space
CY NOV 05-07, 2012
CL CERN, Geneva, SWITZERLAND
SP INFN
HO CERN
DE General theory of relativity; space-based gravity experiments;
scalar-tensor theories
ID GENERAL-RELATIVITY; EQUIVALENCE PRINCIPLE; MISSION; DESIGN
AB General theory of relativity is a standard theory of gravitation; as such, it is used to describe gravity when the problems in astronomy, astrophysics, cosmology, and fundamental physics are concerned. The theory is also relied upon in many modern applications involving spacecraft navigation, geodesy, and time transfer. Here we review the foundations of general relativity and discuss its current empirical status. We describe both the theoretical motivation and the scientific progress that may result from the new generation of high-precision tests that are anticipated in the near future.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Turyshev, SG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM turyshev@jpl.nasa.gov
NR 22
TC 1
Z9 1
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0920-5632
EI 1873-3832
J9 NUCL PHYS B-PROC SUP
JI Nucl. Phys. B-Proc. Suppl.
PD OCT-NOV
PY 2013
VL 243
BP 197
EP 202
DI 10.1016/j.nuclphysbps.2013.09.024
PG 6
WC Physics, Particles & Fields
SC Physics
GA 293GI
UT WOS:000329959000024
ER
PT J
AU Currie, DG
Dell'Agnello, S
Delle Monache, GO
Behr, B
Williams, JG
AF Currie, Douglas G.
Dell'Agnello, Simone
Delle Monache, Giovanni O.
Behr, Bradford
Williams, James G.
TI A Lunar Laser Ranging Retrorefleetor Array for the 21st Century
SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS
LA English
DT Proceedings Paper
CT 4th International Conference on Particle and Fundamental Physics in
Space
CY NOV 05-07, 2012
CL CERN, Geneva, SWITZERLAND
SP INFN
HO CERN
DE Lunar Laser Ranging; Apollo Retroreflectors; General Relativity; Strong
Equivalence Principle; Selenophysics; Lunar Core; Optical/Thermal
Simulation
ID GENERAL-RELATIVITY; MOON; PARAMETERS; PHYSICS; MODELS
AB To date, lunar laser ranging to the Apollo retroreflector arrays, which are still operational after four decades, has produced some of the best tests of General Relativity. Since the ground Observatories have improved their accuracy by a factor of 200, the lunar hardware, due to the lunar librations, now limits the ranging accuracy. The Lunar Laser Ranging Retroreflector Array for the 21st Century program plans to deploy new packages that will improve the ranging accuracy by a factor of ten to one hundred in the next few years.
C1 [Currie, Douglas G.; Behr, Bradford] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Currie, Douglas G.] NASA, Lunar Sci Inst, Moffett Field, CA 94089 USA.
[Dell'Agnello, Simone; Delle Monache, Giovanni O.] Ist Nazl Fis Nucl, Lab Nazl Frascati, I-00044 Frascati, Italy.
[Williams, James G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Currie, DG (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
EM curriedoug@verizon.net
NR 24
TC 5
Z9 5
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0920-5632
EI 1873-3832
J9 NUCL PHYS B-PROC SUP
JI Nucl. Phys. B-Proc. Suppl.
PD OCT-NOV
PY 2013
VL 243
BP 218
EP 228
DI 10.1016/j.nuclphysbps.2013.09.007
PG 11
WC Physics, Particles & Fields
SC Physics
GA 293GI
UT WOS:000329959000026
ER
PT J
AU Abercromby, AFJ
Chappell, SP
Gernhardt, ML
AF Abercromby, Andrew F. J.
Chappell, Steven P.
Gernhardt, Michael L.
TI Desert RATS 2011: Human and robotic exploration of near-Earth asteroids
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Asteroids; Human exploration; Robotics; Operations; Space exploration
vehicle; Analog
AB The Desert Research and Technology Studies (D-RATS) 2011 field test involved the planning and execution of a series of exploration scenarios under operational conditions similar to those expected during a human exploration mission to a near-Earth asteroid (NEA). The focus was on understanding the operations tempo during simulated NEA exploration and the implications of communications latency and limited data bandwidth. Anchoring technologies and sampling techniques were not evaluated due to the immaturity of those technologies and the inability to meaningfully test them at D-RATS. Reduced gravity analogs and simulations are being used to fully evaluate Space Exploration Vehicle (SEV) and extravehicular (EVA) operations and interactions in near-weightlessness at a NEA as part of NASA's integrated analogs program. Hypotheses were tested by planning and performing a series of 1-day simulated exploration excursions comparing test conditions all of which involved a single Deep Space Habitat (DSH) and either 0, 1, or 2 SEVs; 3 or 4 crewmembers; 1 of 2 different communications bandwidths; and a 50-second each-way communications latency between the field site and Houston. Excursions were executed at the Black Point Lava Flow test site with a remote Mission Control Center and Science Support Room at Johnson Space Center (JSC) being operated with 50-second each-way communication latency to the field. Crews were composed of astronauts and professional field geologists. Teams of Mission Operations and Science experts also supported the mission simulations each day. Data were collected separately from the Crew, Mission Operations, and Science teams to assess the test conditions from multiple perspectives. For the operations tested, data indicates practically significant benefits may be realized by including at least one SEV and by including 4 versus 3 crewmembers in the NEA exploration architecture as measured by increased scientific data quality, EVA exploration time, capability assessment ratings, and consensus acceptability ratings provided by Crew, Mission Operations, and Science teams. A combination of text and voice was used to effectively communicate over the communications latency, and increased communication bandwidth yielded a small but practically significant improvement in overall acceptability as rated by the Science team, although the impact of bandwidth on scientific strategic planning and public outreach was not assessed. No effect of increased bandwidth was observed with respect to Crew or Mission Operations team ratings of overall acceptability. (C) 2013 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Abercromby, Andrew F. J.; Chappell, Steven P.] Wyle Integrated Sci & Engn, Houston, TX 77058 USA.
[Gernhardt, Michael L.] NASA, Washington, DC USA.
RP Abercromby, AFJ (reprint author), Wyle Integrated Sci & Engn, 2101 NASA Pkwy,Mail Code Wyle HAC 37C, Houston, TX 77058 USA.
EM andrew.abercromby-1@nasa.gov
NR 17
TC 8
Z9 8
U1 1
U2 14
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT-NOV
PY 2013
VL 91
BP 34
EP 48
DI 10.1016/j.actaastro.2013.05.002
PG 15
WC Engineering, Aerospace
SC Engineering
GA 207GB
UT WOS:000323585800004
ER
PT J
AU Singleterry, RC
AF Singleterry, R. C.
TI Radiation engineering analysis of shielding materials to assess their
ability to protect astronauts in deep space from energetic particle
radiation
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Radiation engineering; Material protection from radiation; Whole body
effective dose equivalent; Radiation engineering analysis; OLTARIS; Long
duration deep space missions
ID ADULT VOXEL PHANTOM; DOSIMETRY
AB An analysis is performed on four typical materials (aluminum, liquid hydrogen, polyethylene, and water) to assess their impact on the length of time an astronaut can stay in deep space and not exceed a design basis radiation exposure of 150 mSv. A large number of heavy lift launches of pure shielding mass are needed to enable long duration, deep space missions to keep astronauts at Or below the exposure value with shielding provided by the vehicle. Therefore, vehicle mass using the assumptions in the paper cannot be the sole shielding mechanism for long duration, deep space missions. As an example, to enable the Mars Design Reference Mission 5.0 with a 400 day transit to and from Mars, not including the 500 day stay on the surface, a minimum of 24 heavy lift launches of polyethylene at 89,375 lbm (40.54 tonnes) each are needed for the 1977 galactic cosmic ray environment. With the assumptions used in this paper, a single heavy lift launch of water or polyethylene can protect astronauts for a 130 day mission before exceeding the exposure value. Liquid hydrogen can only protect the astronauts for 160 days. Even a single launch of pure shielding material cannot protect an astronaut in deep space for more than 180 days using the assumptions adopted in the analysis. It is shown that liquid hydrogen is not the best shielding material for the same mass as polyethylene for missions that last longer than 225 days. Published by Elsevier Ltd. on behalf of IAA.
C1 NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Singleterry, RC (reprint author), NASA Langley Res Ctr, MS 188E, Hampton, VA 23681 USA.
EM robert.c.singleterry@nasa.gov
NR 20
TC 2
Z9 2
U1 3
U2 25
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT-NOV
PY 2013
VL 91
BP 49
EP 54
DI 10.1016/j.actaastro.2013.04.013
PG 6
WC Engineering, Aerospace
SC Engineering
GA 207GB
UT WOS:000323585800005
ER
PT J
AU Love, SG
Reagan, ML
AF Love, Stanley G.
Reagan, Marcum L.
TI Delayed voice communication
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Human space flight; Deep space exploration; Voice communication; Delayed
voice communication; Speed-of-light delay; Space flight analog
AB We present results from simulated deep-space exploration missions that investigated voice communication with significant time delays. The simulations identified many challenges: confusion of sequence, blocked calls, wasted crew time, impaired ability to provide relevant information to the other party, losing track of which messages have reached the other party, weakened rapport between crew and ground, slow response to rapidly changing situations, and reduced situational awareness. These challenges were met in part with additional training; greater attention and foresight; longer, less frequent transmissions; meticulous recordkeeping and timekeeping; and specific alerting and acknowledging calls. Several simulations used both delayed voice and text messaging. Text messaging provided a valuable record of transmissions and allowed messages to be targeted to subsets of the flight and ground crew, but it was a poor choice for high-workload operators such as vehicle drivers and spacewalkers. Even with the foregoing countermeasures, delayed voice communication is difficult. Additional aids such as automatic delay timers and voice-to-text transcription would help. Tests comparing delays of 50 and 300 s unexpectedly revealed that communicating with the shorter delay was just as challenging as with the longer one. Published by Elsevier Ltd. on behalf of IAA.
C1 [Love, Stanley G.; Reagan, Marcum L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Love, SG (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code CB,2101 NASA Pkwy, Houston, TX 77058 USA.
EM stanley.g.love@nasa.gov; marcum.l.reagan@nasa.gov
FU NASA
FX NASA funding supported this work. The authors thank David Korth, Steve
Rader, Vanessa Wyche, and Bernadette Hajek for their helpful feedback.
The authors are also grateful to an anonymous reviewer whose insightful
comments improved this paper.
NR 14
TC 5
Z9 5
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT-NOV
PY 2013
VL 91
BP 89
EP 95
DI 10.1016/j.actaastro.2013.05.003
PG 7
WC Engineering, Aerospace
SC Engineering
GA 207GB
UT WOS:000323585800009
ER
PT J
AU Ryoo, MS
Choi, S
Joung, JH
Lee, JY
Yu, W
AF Ryoo, M. S.
Choi, Sunglok
Joung, Ji Hoon
Lee, Jae-Yeong
Yu, Wonpil
TI Personal driving diary: Automated recognition of driving events from
first-person videos
SO COMPUTER VISION AND IMAGE UNDERSTANDING
LA English
DT Article
DE Personal driving diary; Driving activity recognition; First-person event
detection; Lifelogging
ID REPRESENTATION
AB In this paper, we introduce the concept of personal driving diary. A personal driving diary is a multimedia archive of a person's daily driving experience, describing important driving events of the user with annotated videos. This paper presents an automated system that constructs such multimedia diary by analyzing videos obtained from a vehicle-mounted camera. The proposed system recognizes important interactions between the driving vehicle and the other actors in videos (e.g., accident, overtaking, etc.), and labels them together with its contextual knowledge on the vehicle (e.g., mean velocity) to construct an event log. A decision tree based activity recognizer is designed, detecting driving events of vehicles and pedestrians from the first-person view videos by analyzing their trajectories and spatio-temporal relationships. The constructed diary enables efficient searching and event-based browsing of video clips, which helps the users when retrieving videos of dangerous situations. Our experiment confirms that the proposed system reliably generates driving diaries by annotating the vehicle events learned from training examples. (c) 2013 Elsevier Inc. All rights reserved.
C1 [Ryoo, M. S.] CALTECH, Jet Prop Lab, Mobil & Robot Syst Sect, Pasadena, CA 91109 USA.
[Choi, Sunglok; Lee, Jae-Yeong; Yu, Wonpil] Elect & Telecommun Res Inst, Robot Res Dept, Taejon 305700, South Korea.
[Joung, Ji Hoon] Hyundai Heavy Ind Co Ltd, Engine & Machinery Res Inst, Robot Res Dept, Yongin 446716, South Korea.
RP Ryoo, MS (reprint author), CALTECH, Jet Prop Lab, Mobil & Robot Syst Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mryoo@jpl.nasa.gov
FU R&D program of the Korea Ministry of Knowledge and Economy (MKE); Korea
Evaluation Institute of Industrial Technology (KEIT) [The Development of
Low-cost Autonomous Navigation Systems for a Robot Vehicle in Urban
Environment] [10035354]; R&D Project of Hyundai Heavy Industry Co.,
Ltd.; National Aeronautics and Space Administration
FX This work was supported partly by the R&D program of the Korea Ministry
of Knowledge and Economy (MKE) and the Korea Evaluation Institute of
Industrial Technology (KEIT) [The Development of Low-cost Autonomous
Navigation Systems for a Robot Vehicle in Urban Environment, 10035354].
This work was partially supported by the R&D Project of Hyundai Heavy
Industry Co., Ltd. The writing of this paper was carried out in part at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration.
NR 33
TC 2
Z9 2
U1 2
U2 20
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1077-3142
J9 COMPUT VIS IMAGE UND
JI Comput. Vis. Image Underst.
PD OCT
PY 2013
VL 117
IS 10
BP 1299
EP 1312
DI 10.1016/j.cviu.2013.01.004
PG 14
WC Computer Science, Artificial Intelligence; Engineering, Electrical &
Electronic
SC Computer Science; Engineering
GA 211MW
UT WOS:000323913300009
ER
PT J
AU van der Meer, FP
Davila, CG
AF van der Meer, Frans P.
Davila, Carlos G.
TI Cohesive modeling of transverse cracking in laminates under in-plane
loading with a single layer of elements per ply
SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES
LA English
DT Article
DE Composite laminates; Extended finite element method; Fracture; Cohesive
zone modeling; Transverse cracking; In situ strength
ID MATRIX CRACKING; STATISTICAL-ANALYSIS; DAMAGE MODEL; DELAMINATION;
FRACTURE; FAILURE; GLASS; COMPOSITES; SIMULATION; STRENGTHS
AB This study aims to bridge the gap between classical understanding of transverse cracking in cross-ply laminates and recent computational methods for the modeling of progressive laminate failure. Specifically, the study investigates under what conditions a finite element model with cohesive X-FEM cracks can reproduce the in situ effect for the ply strength. It is shown that it is possible to do so with a single element across the thickness of the ply, provided that the interface stiffness is properly selected. The optimal value for this interface stiffness is derived with an analytical shear lag model. It is also shown that, when the appropriate statistical variation of properties has been applied, models with a single element through the thickness of a ply can predict the density of transverse matrix cracks. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [van der Meer, Frans P.] Delft Univ Technol, Fac Civil Engn & Geosci, NL-2600 GA Delft, Netherlands.
[Davila, Carlos G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP van der Meer, FP (reprint author), Delft Univ Technol, Fac Civil Engn & Geosci, POB 5048, NL-2600 GA Delft, Netherlands.
EM f.p.vandermeer@tudelft.nl; carlos.g.davila@nasa.gov
RI van der Meer, Frans/N-5073-2015
OI van der Meer, Frans/0000-0002-6691-1259
FU Netherlands Technology Foundation (STW) [06623]
FX Financial support from the Netherlands Technology Foundation (STW) under
Grant 06623 is gratefully acknowledged by the first author.
NR 32
TC 8
Z9 8
U1 1
U2 16
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0020-7683
J9 INT J SOLIDS STRUCT
JI Int. J. Solids Struct.
PD OCT
PY 2013
VL 50
IS 20-21
BP 3308
EP 3318
DI 10.1016/j.ijsolstr.2013.06.014
PG 11
WC Mechanics
SC Mechanics
GA 199SI
UT WOS:000323015400022
ER
PT J
AU Barichivich, J
Briffa, KR
Myneni, RB
Osborn, TJ
Melvin, TM
Ciais, P
Piao, SL
Tucker, C
AF Barichivich, Jonathan
Briffa, Keith R.
Myneni, Ranga B.
Osborn, Timothy J.
Melvin, Thomas M.
Ciais, Philippe
Piao, Shilong
Tucker, Compton
TI Large-scale variations in the vegetation growing season and annual cycle
of atmospheric CO2 at high northern latitudes from 1950 to 2011
SO GLOBAL CHANGE BIOLOGY
LA English
DT Review
DE carbon cycle; climate change; NDVI; phenology; vegetation greening
ID CLIMATE-CHANGE; CARBON-DIOXIDE; TIME-SERIES; SNOW-COVER; DATA SET;
PHENOLOGICAL TRANSITIONS; ECOSYSTEM PRODUCTIVITY; SPRING PHENOLOGY;
PLANT PHENOLOGY; BOREAL FORESTS
AB We combine satellite and ground observations during 1950-2011 to study the long-term links between multiple climate (air temperature and cryospheric dynamics) and vegetation (greenness and atmospheric CO2 concentrations) indicators of the growing season of northern ecosystems (>45 degrees N) and their connection with the carbon cycle. During the last three decades, the thermal potential growing season has lengthened by about 10.5days (P<0.01, 1982-2011), which is unprecedented in the context of the past 60years. The overall lengthening has been stronger and more significant in Eurasia (12.6days, P<0.01) than North America (6.2days, P>0.05). The photosynthetic growing season has closely tracked the pace of warming and extension of the potential growing season in spring, but not in autumn when factors such as light and moisture limitation may constrain photosynthesis. The autumnal extension of the photosynthetic growing season since 1982 appears to be about half that of the thermal potential growing season, yielding a smaller lengthening of the photosynthetic growing season (6.7days at the circumpolar scale, P<0.01). Nevertheless, when integrated over the growing season, photosynthetic activity has closely followed the interannual variations and warming trend in cumulative growing season temperatures. This lengthening and intensification of the photosynthetic growing season, manifested principally over Eurasia rather than North America, is associated with a long-term increase (22.2% since 1972, P<0.01) in the amplitude of the CO2 annual cycle at northern latitudes. The springtime extension of the photosynthetic and potential growing seasons has apparently stimulated earlier and stronger net CO2 uptake by northern ecosystems, while the autumnal extension is associated with an earlier net release of CO2 to the atmosphere. These contrasting responses may be critical in determining the impact of continued warming on northern terrestrial ecosystems and the carbon cycle.
C1 [Barichivich, Jonathan; Briffa, Keith R.; Osborn, Timothy J.; Melvin, Thomas M.] Univ E Anglia, Sch Environm Sci, Climat Res Unit, Norwich NR4 7TJ, Norfolk, England.
[Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Ciais, Philippe] Joint Unit CEA CNRS, Lab Climate Sci & Environm LSCE, Gif Sur Yvette, France.
[Piao, Shilong] Peking Univ, Coll Urban & Environm Sci, Beijing 100871, Peoples R China.
[Piao, Shilong] Chinese Acad Sci, Inst Tibetan Plateau Res, Key Lab Alpine & Biodivers, Beijing 100085, Peoples R China.
[Tucker, Compton] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
RP Barichivich, J (reprint author), Univ E Anglia, Sch Environm Sci, Climat Res Unit, Norwich NR4 7TJ, Norfolk, England.
EM j.barichivich@uea.ac.uk
RI Myneni, Ranga/F-5129-2012; Osborn, Timothy/E-9740-2011;
OI Osborn, Timothy/0000-0001-8425-6799; Briffa, Keith/0000-0003-3323-3639
FU Chilean Government under the program Formacion de Capital Humano
Avanzado of CONICYT; UK NERC [NE/G018863/1]
FX We thank Per Jonsson and Lars Eklundh for making available their TIMESAT
routine. We also thank Thomas Estilow of the Global Snow Lab at Rutgers
University and John Caesar of the Met Office Hadley Centre for providing
the most updated snow-cover and temperature data, respectively. JB was
supported by doctoral scholarship from the Chilean Government under the
program Formacion de Capital Humano Avanzado of CONICYT. KRB, TJO, and
TMM acknowledge support from UK NERC (under grant NE/G018863/1).
NR 109
TC 64
Z9 66
U1 8
U2 191
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
EI 1365-2486
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD OCT
PY 2013
VL 19
IS 10
BP 3167
EP 3183
DI 10.1111/gcb.12283
PG 17
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 210OS
UT WOS:000323844200023
PM 23749553
ER
PT J
AU Mehta, SK
Tyring, SK
Cohrs, RJ
Gilden, D
Feiveson, AH
Lechler, KJ
Pierson, DL
AF Mehta, Satish K.
Tyring, Stephen K.
Cohrs, Randall J.
Gilden, Don
Feiveson, Alan H.
Lechler, Kayla J.
Pierson, Duane L.
TI Rapid and sensitive detection of varicella zoster virus in saliva of
patients with herpes zoster
SO JOURNAL OF VIROLOGICAL METHODS
LA English
DT Article
DE Saliva; Varicella zoster virus; DNA; PCR
ID REACTIVATION
AB VZV reactivation produces zoster (shingles) which may be further complicated by meningoencephalitis, myelopathy, vasculopathy and multiple ocular disorders. Importantly, these neurological and ocular complications of VZV reactivation can occur without rash. In such instances, virological verification relies on detection of VZV DNA or anti-VZV IgG antibody in cerebrospinal fluid (CSF), or less often, the presence of VZV DNA in blood mononuclear cells or anti-VZV IgM antibody in serum or CSF. If VZV were readily detected in other tissue samples (e.g., saliva or tears) in patients with neurological disease in the absence of rash and shown to correlate with the standard tests listed above, more invasive tests such as lumbar puncture might be obviated.
In patients with acute herpes zoster, the yield of cell DNA was greater in saliva collected by passive drool or synthetic swab than by cotton swab. The time to process saliva from collection to obtaining DNA was 1 h. VZV DNA was present exclusively in the pelleted fraction of saliva and was found in 100% of patients before antiviral treatment. This rapid sensitive method can be applied readily to saliva from humans with neurologic and other disease that might be caused by VZV in the absence of rash. (c) 2013 Elsevier B.V. All rights reserved.
C1 [Mehta, Satish K.] Enterprise Advisory Serv Inc, Houston, TX 77598 USA.
[Tyring, Stephen K.] Univ Texas Hlth Sci Ctr Houston, Dept Dermatol, Houston, TX 77598 USA.
[Cohrs, Randall J.; Gilden, Don] Univ Colorado, Sch Med, Dept Neurol, Aurora, CO 80045 USA.
[Gilden, Don] Univ Colorado, Sch Med, Dept Microbiol, Aurora, CO 80045 USA.
[Feiveson, Alan H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Lechler, Kayla J.; Pierson, Duane L.] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Associates, Houston, TX 77058 USA.
[Lechler, Kayla J.; Pierson, Duane L.] NASA, Lyndon B Johnson Space Ctr, Dept Microbiol, Houston, TX 77058 USA.
RP Gilden, D (reprint author), Univ Colorado, Sch Med, Dept Neurol, Aurora, CO 80045 USA.
EM satish.k.mehta@nasa.gov; styring@ccstexas.com;
randall.cohrs@ucdenver.edu; don.gilden@ucdenver.edu;
alan.h.feiveson@nasa.gov; kayla.j.lechler@nasa.gov;
duane.l.piersonl@nasa.gov
FU NASA [111-30-10-03, 111-30-10-06]; Public Health Service from the
National Institutes of Health [AG032958, AG006127]
FX This work was supported by,NASA grants 111-30-10-03, 111-30-10-06 to DLP
and by Public Health Service grants AG032958 (D.G., R.J.C.) and AG006127
(D.G.) from the National Institutes of Health. We thank Marina Hoffman
for editorial review and Lori DePriest for manuscript preparation.
NR 8
TC 3
Z9 3
U1 2
U2 17
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0166-0934
J9 J VIROL METHODS
JI J. Virol. Methods
PD OCT
PY 2013
VL 193
IS 1
BP 128
EP 130
DI 10.1016/j.jviromet.2013.05.019
PG 3
WC Biochemical Research Methods; Biotechnology & Applied Microbiology;
Virology
SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology;
Virology
GA 204JR
UT WOS:000323362100019
PM 23747545
ER
PT J
AU Eppler, D
Bleacher, J
AF Eppler, Dean
Bleacher, Jacob
TI D-RATS mission results
SO ACTA ASTRONAUTICA
LA English
DT Editorial Material
C1 [Eppler, Dean] NASA, Lyndon B Johnson Space Ctr, Washington, DC 20546 USA.
[Bleacher, Jacob] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Eppler, D (reprint author), NASA, Lyndon B Johnson Space Ctr, Washington, DC 20546 USA.
EM Dean.B.Eppler@nasa.gov
RI Bleacher, Jacob/D-1051-2012
OI Bleacher, Jacob/0000-0002-8499-4828
NR 0
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 181
EP 181
DI 10.1016/j.actaastro.2013.04.012
PG 1
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100001
ER
PT J
AU Ross, A
Kosmo, J
Janoiko, B
AF Ross, Amy
Kosmo, Joseph
Janoiko, Barbara
TI Historical synopses of desert RATS 1997-2010 and a preview of desert
RATS 2011
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Analog; Space suit; Planetary exploration; Field test; EVA; SEV; Suit
port; RATS
AB Desert RATS objectives, hardware, locations, and participants have changed over time. This paper provides historical perspective on the original motivations for the Desert RATS analog, and an overview of the changes in RATS over time. The lessons learned from each year are synopsized. Finally, a preview of Desert RATS 2011 tests is included. Published by Elsevier Ltd. on behalf of IAA.
C1 [Ross, Amy; Kosmo, Joseph; Janoiko, Barbara] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Ross, A (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code EC5,2101 NASA Pkwy, Houston, TX 77058 USA.
EM Amy.j.ross@nasa.gov
NR 14
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U1 1
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 182
EP 202
DI 10.1016/j.actaastro.2012.02.003
PG 21
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100002
ER
PT J
AU Abercromby, AFJ
Gernhardt, ML
Jadwick, J
AF Abercromby, Andrew F. J.
Gernhardt, Michael L.
Jadwick, Jennifer
TI Evaluation of dual multi-mission space exploration vehicle operations
during simulated planetary surface exploration
SO ACTA ASTRONAUTICA
LA English
DT Article
DE MMSEV; Rover; Exploration; Lunar; Analog; Simulation
AB Introduction: A pair of small pressurized rovers (multi-mission space exploration vehicles, or MMSEVs) is at the center of the Global Point-of-Departure architecture for future human lunar exploration. Simultaneous operation of multiple crewed surface assets should maximize productive crew time, minimize overhead, and preserve contingency return paths.
Methods: A 14-day mission simulation was conducted in the Arizona desert as part of NASA's 2010 Desert Research and Technology Studies (DRATS) field test. The simulation involved two MMSEV earth-gravity prototypes performing geological exploration under varied operational modes affecting both the extent to which the MMSEVs must maintain real-time communications with the mission control center (Continuous [CC] versus Twice-a-Day [2/D]) and their proximity to each other (Lead-and-Follow [L&F] versus Divide-and-Conquer [D&C]). As part of a minimalist lunar architecture, no communication relay satellites were assumed. Two-person crews (an astronaut and a field geologist) operated each MMSEV, day and night, throughout the entire 14-day mission, only leaving via the suit ports to perform simulated extravehicular activities. Metrics and qualitative observations enabled evaluation of the extent to which the operating modes affected productivity and scientific data quality (SDQ).
Results and discussion: SDQ was greater during CC mode than during 2/D mode; metrics showed a marginal increase while qualitative assessments suggested a practically significant difference. For the communications architecture evaluated, significantly more crew time (14% per day) was required to maintain communications during D&C than during L&F (5%) or 2/D (2%), increasing the time required to complete all traverse objectives. Situational awareness of the other vehicle's location, activities, and contingency return constraints were qualitatively enhanced during L&F and 2/D modes due to line-of-sight and direct MMSEV-to-MMSEV communication. Future testing will evaluate approaches to operating without real-time space-to-earth communications and will include quantitative evaluation and comparison of the efficacy of mission operations, science operations, and public outreach operations. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Abercromby, Andrew F. J.; Jadwick, Jennifer] Wyle Integrated Sci & Engn Grp, Houston, TX USA.
[Gernhardt, Michael L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Abercromby, AFJ (reprint author), Wyle Integrated Sci & Engn Grp, Houston, TX USA.
EM andrew.abercromby-l@nasa.gov
NR 9
TC 3
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U1 0
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 203
EP 214
DI 10.1016/j.actaastro.2012.02.022
PG 12
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100003
ER
PT J
AU Bell, ER
Badillo, V
Coan, D
Johnson, K
Ney, Z
Rosenbaum, M
Smart, T
Stone, J
Stueber, R
Welsh, D
Guirgis, P
Looper, C
McDaniel, R
AF Bell, Ernest R., Jr.
Badillo, Victor
Coan, David
Johnson, Kieth
Ney, Zane
Rosenbaum, Megan
Smart, Tifanie
Stone, Jeffry
Stueber, Ronald
Welsh, Daren
Guirgis, Peggy
Looper, Chris
McDaniel, Randall
TI Mission control team structure and operational lessons learned from the
2009 and 2010 NASA desert RATS simulated lunar exploration field tests
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Desert RATS; Lunar analog; Lunar exploration; Mission operations; Flight
control; EVA
AB The NASA Desert Research and Technology Studies (Desert RATS) is an annual field test of advanced concepts, prototype hardware, and potential modes of operation to be used on human planetary surface space exploration missions. For the 2009 and 2010 NASA Desert RATS field tests, various engineering concepts and operational exercises were incorporated into mission timelines with the focus of the majority of daily operations being on simulated lunar geological field operations and executed in a manner similar to current Space Shuttle and International Space Station missions. The field test for 2009 involved a two week lunar exploration simulation utilizing a two-man rover. The 2010 Desert RATS field test took this two week simulation further by incorporating a second two-man rover working in tandem with the 2009 rover, as well as including docked operations with a Pressurized Excursion Module (PEM). Personnel for the field test included the crew, a mission management team, engineering teams, a science team, and the mission operations team. The mission operations team served as the core of the Desert RATS mission control team and included certified NASA Mission Operations Directorate (MOD) flight controllers, former flight controllers, and astronaut personnel. The backgrounds of the flight controllers were in the areas of Extravehicular Activity (EVA), onboard mechanical systems and maintenance, robotics, timeline planning (OpsPlan), and space-craft communicator (Capcom). With the simulated EVA operations, mechanized operations (the rover), and expectations of replanning, these flight control disciplines were especially well suited for the execution of the 2009 and 2010 Desert RATS field tests. The inclusion of an operations team has provided the added benefit of giving NASA mission operations flight control personnel the opportunity to begin examining operational mission control techniques, team compositions, and mission scenarios. This also gave the mission operations team the opportunity to gain insight into functional hardware requirements via lessons learned from executing the Desert RATS field test missions. This paper will detail the mission control team structure that was used during the 2009 and 2010 Desert RATS Lunar analog missions. It will also present a number of the lessons learned by the operations team during these field tests. Major lessons learned involved Mission Control Center (MCC) operations, pre-mission planning and training processes, procedure requirements, communication requirements, and logistic support for analogs. This knowledge will be applied to future Desert RATS field tests, and other Earth based analog testing for space exploration, to continue the evolution of manned space operations in preparation for human planetary exploration. It is important that operational knowledge for human space exploration missions be obtained during Earth-bound field tests to the greatest extent possible. This allows operations personnel the ability to examine various flight control and crew operations scenarios in preparation for actual space missions. (C) 2013 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Bell, Ernest R., Jr.; Badillo, Victor; Coan, David; Johnson, Kieth; Ney, Zane; Rosenbaum, Megan; Smart, Tifanie; Stone, Jeffry; Stueber, Ronald; Welsh, Daren] NASA, United Space Alliance LLC, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Guirgis, Peggy; Looper, Chris; McDaniel, Randall] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Bell, ER (reprint author), NASA, United Space Alliance LLC, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM ernest.r.bell@nasa.gov
NR 8
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U1 3
U2 22
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 215
EP 223
DI 10.1016/j.actaastro.2012.11.020
PG 9
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100004
ER
PT J
AU Eppler, D
Adams, B
Archer, D
Baiden, G
Brown, A
Carey, W
Cohen, B
Condit, C
Evans, C
Fortezzo, C
Garry, B
Graff, T
Gruener, J
Heldmann, J
Hodges, K
Horz, F
Hurtado, J
Hynek, B
Isaacson, P
Juranek, C
Klaus, K
Kring, D
Lanza, N
Lederer, S
Lofgren, G
Marinova, M
May, L
Meyer, J
Ming, D
Monteleone, B
Morisset, C
Noble, S
Rampe, E
Rice, J
Schutt, J
Skinner, J
Tewksbury-Christle, CM
Tewksbury, BJ
Vaughan, A
Yingst, A
Young, K
AF Eppler, Dean
Adams, Byron
Archer, Doug
Baiden, Greg
Brown, Adrian
Carey, William
Cohen, Barbara
Condit, Chris
Evans, Cindy
Fortezzo, Corey
Garry, Brent
Graff, Trevor
Gruener, John
Heldmann, Jennifer
Hodges, Kip
Hoerz, Friedrich
Hurtado, Jose
Hynek, Brian
Isaacson, Peter
Juranek, Catherine
Klaus, Kurt
Kring, David
Lanza, Nina
Lederer, Susan
Lofgren, Gary
Marinova, Margarita
May, Lisa
Meyer, Jonathan
Ming, Doug
Monteleone, Brian
Morisset, Caroline
Noble, Sarah
Rampe, Elizabeth
Rice, James
Schutt, John
Skinner, James
Tewksbury-Christle, Carolyn M.
Tewksbury, Barbara J.
Vaughan, Alicia
Yingst, Aileen
Young, Kelsey
TI Desert Research and Technology Studies (DRATS) 2010 science operations:
Operational approaches and lessons learned for managing science during
human planetary surface missions
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Planetary surface operations; Analog testing; Science operations;
Planetary science; Metric evaluation
AB Desert Research and Technology Studies (Desert RATS) is a multi-year series of hardware and operations tests carried out annually in the high desert of Arizona on the San Francisco Volcanic Field. These activities are designed to exercise planetary surface hardware and operations in conditions where long-distance, multi-day roving is achievable, and they allow NASA to evaluate different mission concepts and approaches in an environment less costly and more forgiving than space. The results from the RATS tests allow selection of potential operational approaches to planetary surface exploration prior to making commitments to specific flight and mission hardware development. In previous RATS operations, the Science Support Room has operated largely in an advisory role, an approach that was driven by the need to provide a loose science mission framework that would underpin the engineering tests. However, the extensive nature of the traverse operations for 2010 expanded the role of the science operations and tested specific operational approaches. Science mission operations approaches from the Apollo and Mars-Phoenix missions were merged to become the baseline for this test. Six days of traverse operations were conducted during each week of the 2-week test, with three traverse days each week conducted with voice and data communications continuously available, and three traverse days conducted with only two 1-hour communications periods per day. Within this framework, the team evaluated integrated science operations management using real-time, tactical science operations to oversee daily crew activities, and strategic level evaluations of science data and daily traverse results during a post-traverse planning shift. During continuous communications, both tactical and strategic teams were employed. On days when communications were reduced to only two communications periods per day, only a strategic team was employed. The Science Operations Team found that, if communications are good and down-linking of science data is ensured, high quality science returns is possible regardless of communications. What is absent from reduced communications is the scientific interaction between the crew on the planet and the scientists on the ground. These scientific interactions were a critical part of the science process and significantly improved mission science return over reduced communications conditions. The test also showed that the quality of science return is not measurable by simple numerical quantities but is, in fact, based on strongly non-quantifiable factors, such as the interactions between the crew and the Science Operations Teams. Although the metric evaluation data suggested some trends, there was not sufficient granularity in the data or specificity in the metrics to allow those trends to be understood on numerical data alone. Published by Elsevier Ltd. on behalf of IAA.
C1 [Eppler, Dean; Archer, Doug; Evans, Cindy; Graff, Trevor; Gruener, John; Hoerz, Friedrich; Lederer, Susan; Lofgren, Gary; Ming, Doug] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Brown, Adrian; Heldmann, Jennifer; Marinova, Margarita] NASA, Ames Res Ctr, Houston, TX 77058 USA.
[Noble, Sarah; Rice, James] NASA, Goddard Space Flight Ctr, Houston, TX 77058 USA.
[Fortezzo, Corey; Skinner, James; Vaughan, Alicia] US Geol Survey, Flagstaff, AZ 86001 USA.
[Hynek, Brian] Univ Colorado, Boulder, CO 80309 USA.
[Hurtado, Jose; Meyer, Jonathan] Univ Texas El Paso, El Paso, TX 79968 USA.
[Klaus, Kurt] Boeing Co, Houston, DC USA.
[Isaacson, Peter] Brown Univ, Providence, RI 02912 USA.
[Adams, Byron; Hodges, Kip; Monteleone, Brian; Rampe, Elizabeth; Young, Kelsey] Arizona State Univ, Tempe, AZ 85287 USA.
[Cohen, Barbara] NASA, George C Marshall Space Flight Ctr, Houston, TX 77058 USA.
[Lanza, Nina] Univ New Mexico, Albuquerque, NM 87131 USA.
[Tewksbury, Barbara J.] Hamilton Coll, Clinton, NY 13323 USA.
[Baiden, Greg] Laurentian Univ, Sudbury, ON P3E 2C6, Canada.
[Condit, Chris] Univ Massachusetts, Amherst, MA 01003 USA.
[Juranek, Catherine] No Arizona Univ, Flagstaff, AZ 86011 USA.
RP Eppler, D (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code KX,2101 NASA Pkwy, Houston, TX 77058 USA.
EM dean.b.eppler@nasa.gov
RI Fortezzo, Corey/J-3768-2013; Hodges, Kip/A-7992-2009; Noble,
Sarah/D-7614-2012; Garry, Brent/I-5920-2013; Skinner, James/M-7966-2014;
Adams, Byron/I-4243-2015
OI Hodges, Kip/0000-0003-2805-8899; Adams, Byron/0000-0001-8219-3544
FU NASA
FX The Science Team acknowledges exceptional work by all members of the
Desert RATS Team, in particular Mr. Joseph Kosmo and Ms. Barbara Janoiko
of the NASA-JSC Crew and Thermal Systems Division; the Rover Team,
specifically Dr. William Bluethmann and Ms. Jodi Graf of the NASA-JSC
Robotics Division; the Communications Team, specifically Mr. Marc
Seibert, Mr. Michael Downs and Mr. Michael Miller of the NASA-Kennedy
Space Center, and rover crewmembers, Dr. Jose Hurtado of the University
of Texas-El Paso, Dr. Jake Bleacher of NASA-Goddard Spaceflight Center,
Ms. Kelsey Young of Arizona State University, Dr. Michael Gernhardt of
the NASA-JSC Astronaut Office, Dr. Jim Rice of NASA-Goddard Spaceflight
Center, Mr. Chris Looper of the NASA-JSC Astronaut Office, Mr. Aaron
Hulce of the NASA-JSC Robotics Division and (presently) the United
States Navy, Dr. Stephanie Wilson of the NASA-JSC Astronaut Office and
Dr. Stan Love of the NASA-JSC Astronaut Office. In addition, the EVA
Information Systems in the backpacks and the Giga-Pan cameras on the
rovers were of critical importance to the Strategic Team's work, and Mr.
Scott Bleisath and Dr. Matthew Deans and their respective teams are to
be commended for their efforts. Lastly, the science team acknowledges
the tireless work of "Black Point Base Camp Mayor" Mr. Darby Magruder,
robotics engineer, logistician, and general miracle worker who made sure
the TSOT had what it needed to get the job done in the field. Each of
these groups worked long hours away from home for many weeks, and
without their efforts, the Desert RATS mission would still be on the
back lot at Johnson Space Center, playing pinochle in the science
trailer for 14 days. The SSOT members acknowledge the staff of the
Embassy Suites in Flagstaff, AZ, for turning over their conference
facility nightly to the team for its work and deliberations. The
principal author acknowledges Dr. Wendell Mendell and NASA's
Constellation Program, which provided the funding to assemble a
world-class science team. Lastly, thanks go to Ms. Shelly Kelly of the
University of Houston-Clear Lake Space History Archives and Ms. Linda
Chappel of the Lunar and Planetary Institute Library for discovering
"lost" documents concerning the conduct of science mission operations on
Apollo. This paper was improved significantly by comprehensive reviews
by Dr. Jim Head and an anonymous reviewer.
NR 14
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 224
EP 241
DI 10.1016/j.actaastro.2012.03.009
PG 18
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100005
ER
PT J
AU Horz, F
Lofgren, GE
Gruener, JE
Eppler, DB
Skinner, JA
Fortezzo, CM
Graf, JS
Bluethmann, WJ
Seibert, MA
Bell, ER
AF Hoerz, Friedrich
Lofgren, Gary E.
Gruener, John E.
Eppler, Dean B.
Skinner, James A., Jr.
Fortezzo, Corey M.
Graf, Jodi S.
Bluethmann, William J.
Seibert, Marc A.
Bell, Ernest R.
TI The traverse planning process for D-RATS 2010
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Surface exploration; Rover; Mission operations; EVA; Ground support;
Communications
AB This report describes the traverse planning process for the Desert Research and Technology Studies (D-RATS) 2010 field simulation of a conceptual 14-day planetary mission. This activity took place between August 23 and September 17, 2010 in the San Francisco Volcanic Field, Arizona. It focused on the utilization of two pressurized rovers and a ground-based communication system, as well as on the development of mission operation concepts for long duration, dual-rover missions. The early planning process began some 12 months prior to the actual field tests and defined the first order engineering-, flight operations, and science objectives. The detailed implementation and refinement of these objectives took place over the ensuing 10 months, resulting in a large number of technical and operational constraints that affected the actual traverse route or the cumulative Extravehicular Activity (EVA) time available for detailed field observations. The science planning proceeded from the generation of photogeologic maps of the test area, to the establishment of prioritized science objectives and associated candidate sites for detailed field exploration. The combination of operational constraints and science objectives resulted in the final design of traverse routes and time lines for each of the 24 traverses needed to support 12 field days by two rovers. Examples of daily traverses will be given that will hopefully illustrate that the design of long duration, long distance planetary traverses is a highly interdisciplinary and time-consuming collaboration between diverse engineers, flight operations personnel, human factors interests, and planetary scientists. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Hoerz, Friedrich] LZ Technol ESCG, Houston, TX 77058 USA.
[Lofgren, Gary E.] NASA, Lyndon B Johnson Space Ctr, Off Curator, Houston, TX 77058 USA.
[Gruener, John E.; Eppler, Dean B.] NASA, Lyndon B Johnson Space Ctr, Human Explorat Off, Houston, TX 77058 USA.
[Skinner, James A., Jr.; Fortezzo, Corey M.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Graf, Jodi S.; Bluethmann, William J.] NASA, Lyndon B Johnson Space Ctr, Software & Robot Div, Houston, TX 77058 USA.
[Seibert, Marc A.] NASA, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA.
[Bell, Ernest R.] United Space Alliance LLC, Johnson Space Ctr, Houston, TX 77058 USA.
RP Horz, F (reprint author), LZ Technol ESCG, 2224 Bay Area Blvd, Houston, TX 77058 USA.
EM friedrich.p.horz@nasa.gov
RI Fortezzo, Corey/J-3768-2013
NR 2
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U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 254
EP 267
DI 10.1016/j.actaastro.2012.02.008
PG 14
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100007
ER
PT J
AU Lee, SY
Lees, D
Cohen, T
Allan, M
Deans, M
Morse, T
Park, E
Smith, T
AF Lee, Susan Y.
Lees, David
Cohen, Tamar
Allan, Mark
Deans, Matthew
Morse, Theodore
Park, Eric
Smith, Trey
TI Reusable science tools for analog exploration missions: xGDS Web Tools,
VERVE, and Gigapan Voyage
SO ACTA ASTRONAUTICA
LA English
DT Article
DE NASA; Planetary analogs; Intelligent Robotics Group; Robotic Field Test;
Desert Research and Technology Studies; Ground Data Systems; Gigapan
Voyage; VERVE
AB The Exploration Ground Data Systems (xGDS) project led by the Intelligent Robotics Group (IRG) at NASA Ames Research Center creates software tools to support multiple NASA-led planetary analog field experiments. The two primary tools that fall under the xGDS umbrella are the xGDS Web Tools (xGDS-WT) and Visual Environment for Remote Virtual Exploration (VERVE). IRG has also developed a hardware and software system that is closely integrated with our xGDS tools and is used in multiple field experiments called Gigapan Voyage. xGDS-WT, VERVE, and Gigapan Voyage are examples of IRG projects that improve the ratio of science return versus development effort by creating generic and reusable tools that leverage existing technologies in both hardware and software.
xGDS Web Tools provides software for gathering and organizing mission data for science and engineering operations, including tools for planning traverses, monitoring autonomous or piloted vehicles, visualization, documentation, analysis, and search. VERVE provides high performance three dimensional (3D) user interfaces used by scientists, robot operators, and mission planners to visualize robot data in real time. Gigapan Voyage is a gigapixel image capturing and processing tool that improves situational awareness and scientific exploration in human and robotic analog missions. All of these technologies emphasize software reuse and leverage open source and/or commercial-off-the-shelf tools to greatly improve the utility and reduce the development and operational cost of future similar technologies.
Over the past several years these technologies have been used in many NASA-led robotic field campaigns including the Desert Research and Technology Studies (DRATS), the Pavilion Lake Research Project (PLRP), the K10 Robotic Follow-Up tests, and most recently we have become involved in the NASA Extreme Environment Mission Operations (NEEMO) field experiments. A major objective of these joint robot and crew experiments is to improve NASAs understanding of how to most effectively execute and increase science return from exploration missions. This paper focuses on an integrated suite of xGDS software and compatible hardware tools: xGDS Web Tools, VERVE, and Gigapan Voyage, how they are used, and the design decisions that were made to allow them to be easily developed, integrated, tested, and reused by multiple NASA field experiments and robotic platforms. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Lees, David; Morse, Theodore; Park, Eric; Smith, Trey] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA.
[Deans, Matthew] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM susan.y.lee@nasa.gov; david.s.lees@nasa.gov; tamar.e.cohen@nasa.gov;
mark.b.allan@nasa.gov; matthew.deans@nasa.gov;
theodore.f.morse@nasa.gov; eric.park@nasa.gov; trey.smith@nasa.gov
FU NASA Ames Research Center; Johnson Space Center; NASA
FX This work was supported in part by NASA Ames Research Center and Johnson
Space Center under the Human Robotic Systems Project and sponsored by
the NASA Exploration Technology Development Program.
NR 16
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SN 0094-5765
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JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 268
EP 288
DI 10.1016/j.actaastro.2012.01.002
PG 21
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100008
ER
PT J
AU Evans, CA
Calaway, MJ
Bell, MS
Young, KE
AF Evans, Cynthia A.
Calaway, Michael J.
Bell, Mary Sue
Young, Kelsey E.
TI GeoLab-A habitat-based laboratory for preliminary examination of
geological samples
SO ACTA ASTRONAUTICA
LA English
DT Article
DE GeoLab; Glovebox; Astromaterials; Curation; Exploration; Analog
AB GeoLab is a prototype geological laboratory designed for deployment and testing during NASA's analog demonstrations. Scientists at NASA's Johnson Space Center (JSC) built GeoLab as part of a technology project to support the development of science operational concepts for future planetary surface missions. It was integrated into NASA's Habitat Demonstration Unit 1 - Pressurized Excursion Module (HDU1-PEM), a first generation exploration habitat test bed.
As a test bed, GeoLab provides a high fidelity working space for crewmembers to perform preliminary examination and characterization of geologic samples. The GeoLab concept builds from the hardware and cleanroom protocols used in JSC's Astromaterials Sample Curation laboratories. The main hardware component of the GeoLab is a custom-built glovebox, constructed from stainless steel and polycarbonate, and built to provide a positive pressure nitrogen environment. The glovebox is mounted onto the habitat's structural ribs; the unique shape (trapezoidal prism) fits within a pie-shaped section of the cylindrical habitat. A key innovation of GeoLab is the mechanism for transferring samples into the glovebox: three antechambers (airlocks) that pass through the shell of the habitat. These antechambers allow geologic samples to enter and exit the main glovebox chamber directly from (and to) the outside, thereby controlling contamination from inside the habitat. The glovebox is configured to include imaging systems, instrumentation, and computer controls. The first field trials tested a simple configuration including a microscope, a commercially available handheld X-ray Fluorescence instrument, network cameras, and simple sample handling tools inside the glovebox.
We present results from the initial field trials of GeoLab during the 2010 Desert Research and Technology Studies (Desert RATS) planetary analog test near Flagstaff, AZ. These field tests examined the general operations of the GeoLab hardware and the crew interfaces for operating the laboratory. GeoLab operations also resulted in the preliminary examination of selected samples for Desert RATS science team decisions regarding prioritization of samples. Published by Elsevier Ltd. on behalf of IAA.
C1 [Evans, Cynthia A.] NASA Johnson Space Ctr, Astromat Acquisit & Curat Off, Houston, TX 77058 USA.
[Calaway, Michael J.; Bell, Mary Sue] NASA Johnson Space Ctr, Jacobs Technol Engn & Sci Contract Grp, Astromat Acquisit & Curat Off, Houston, TX 77058 USA.
[Young, Kelsey E.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Evans, CA (reprint author), NASA Johnson Space Ctr, Astromat Acquisit & Curat Off, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM cindy.evans-1@nasa.gov; michael.calaway@nasa.gov; mary.s.bell@nasa.gov;
Kelsey.E.Young@asu.edu
FU JSC Technology funds; NASA [NNX10AK72H]
FX The GeoLab project was supported by JSC Technology funds administered by
the JSC Advanced Planning Office. We would like to acknowledge our
partnership with the entire Habitat Demonstrations Unit Team, and extend
special thanks to the HDU management team (K. Kennedy, T. Tri, T. Gill,
S. Howe), and the avionics and software teams for continuing operational
support. We also acknowledge the Desert RATS Managers (Joe Kosmo and
Barbara Janoiko), the Mission Operations team, the Science Team and the
GeoLab operators (the 2010 Desert RATS crew - Kelsey Young, Stephanie
Wilson, Jose Hurtado, Aaron Hulse, Jake Bleacher, Stan Love, Jim Rice
and Chris Looper). K. Young was supported through funding from the NASA
Graduate Student Researchers Program Grant #NNX10AK72H.
NR 26
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SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 289
EP 300
DI 10.1016/j.actaastro.2011.12.008
PG 12
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100009
ER
PT J
AU Paul, HL
AF Paul, Heather L.
TI Desert Research and Technology Studies (DRATS) 2010 Education and Public
Outreach (EPO)
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Education; Outreach; Media; Social media; Participatory Exploration
AB The Exploration Systems Mission Directorate, Directorate Integration Office conducts analog field test activities, such as Desert Research and Technology Studies (DRATS), to validate exploration system architecture concepts and conduct technology demonstrations. Education and Public Outreach (EPO) activities have been a part of DRATS missions in the past to engage students, educators, and the general public in analog activities. However, in 2010, for the first time, EPO was elevated as a principal task for the mission and metrics were collected for all EPO activities. EPO activities were planned well in advance of the mission, with emphasis on creating a multitude of activities to attract students of all ages. Web-based and social media interaction between August 31 and September 14, 2010 resulted in 62,260 DRATS Flickr views: 10,906 views of DRATS videos on YouTube; 1,483 new DRATS Twitter followers; and a 111% increase in DRATS Facebook fan interactions. Over 7,000 outreach participants were directly involved in the DRATS 2010 analog mission via student visitations at both the integrated dry-runs prior to the field mission and during the field mission; by participating in live, interactive webcasts and virtual events; and online voting to determine a traverse site as part of the NASA initiative for Participatory Exploration (PE). (C) 2013 Published by Elsevier Ltd. on behalf of IAA.
C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Paul, HL (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mail Code EC8, Houston, TX 77058 USA.
EM heather.l.paul@nasa.gov
NR 8
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SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 301
EP 310
DI 10.1016/j.actaastro.2012.05.027
PG 10
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100010
ER
PT J
AU Yingst, RA
Cohen, BA
Ming, DW
Eppler, DB
AF Yingst, R. A.
Cohen, B. A.
Ming, D. W.
Eppler, D. B.
TI Comparing Apollo and Mars Exploration Rover (MER)/phoenix operations
paradigms for human exploration during NASA Desert-RATS science
operations
SO ACTA ASTRONAUTICA
LA English
DT Article
DE MER; Science operations; Apollo; Phoenix
AB The Desert Research and Technology Studies (D-RATS) field tested two models of human-in-the-loop remote field geology: one based on the Apollo science backroom that integrated tactical and strategic decisions, and one that separated tactical and strategic processes as utilized during the Mars Exploration Rovers (MER) and Mars Phoenix Scout missions. The 2010 D-RATS field test was the first attempt at integrating best practices from these two models, to determine how best to maximize science return from future missions.
The Apollo model was utilized in 2008 and 2009 as a way to integrate science into field analog studies; the model allowed for real time communications between the crew on the surface and the scientists in the backroom. This model greatly improved efficiency of field operations and scientific return, but did not allow sufficient time for hypotheses to mature to the point where they could inform operations. The MER/Phoenix model, adapted for the 2010 D-RATS test, divided the responsibilities and processes of tactical science and strategic science. This division provided opportunities to discuss science results in greater detail so that the overall planning of science observations could be iterative rather than static. However, because of the nearly complete separation of the two science teams, there was a great deal of repeated effort as the strategic team had no prior knowledge of the tactical process and the observations that led to certain tactical decisions.
Lessons learned from 2010 D-RATS science operations include: (1) well-trained geologists on the crew and a science backroom with which that crew can interact are both critical components for maximizing science return; (2) sufficient time or another mechanism that increases time available to be spent on science analysis must be built into the system to allow free rein to the scientific process; (3) data flow must be improved so that time is not wasted in repetitive review of acquired datasets; and (4) stable, high-fidelity communication must be available for any science activity where humans are in the loop. (C) 2011 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Yingst, R. A.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Cohen, B. A.] NASA Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Ming, D. W.; Eppler, D. B.] NASA Johnson Spaceflight Ctr, Houston, TX 77058 USA.
RP Yingst, RA (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
EM yingst@psi.edu; barbara.a.cohen@nasa.gov; douglas.w.ming@nasa.gov;
dean.b.eppler@nasa.gov
FU NASA MMAMA [NNX09AV96G]
FX The authors would like to thank the engineers and scientists with whom
we had the honor to work during the D-RATS field work. Partial support
of this work was provided by NASA MMAMA Grant #NNX09AV96G to RAY. BAC
was supported in the 2009 D-RATS experience by the Field Science Analog
Testing program. Discussions with Dr. Janet Vertesi formed the
beginnings of this manuscript.
NR 18
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SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 311
EP 317
DI 10.1016/j.actaastro.2011.10.001
PG 7
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100011
ER
PT J
AU Love, SG
Bleacher, JE
AF Love, Stanley G.
Bleacher, Jacob E.
TI Crew roles and interactions in scientific space exploration
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Astronaut training; Cockpit resource management; Crew tasking; Group
interaction; Human space flight; Space flight analog
AB Future piloted space exploration missions will focus more on science than engineering, a change which will challenge existing concepts for flight crew tasking and demand that participants with contrasting skills, values, and backgrounds learn to cooperate as equals. In terrestrial space flight analogs such as Desert Research And Technology Studies, engineers, pilots, and scientists can practice working together, taking advantage of the full breadth of all team members' training to produce harmonious, effective missions that maximize the time and attention the crew can devote to science. This paper presents, in a format usable as a reference by participants in the field, a successfully tested crew interaction model for such missions. The model builds upon the basic framework of a scientific field expedition by adding proven concepts from aviation and human space flight, including expeditionary behavior and cockpit resource management, cooperative crew tasking and adaptive leadership and followership, formal techniques for radio communication, and increased attention to operational considerations. The crews of future space flight analogs can use this model to demonstrate effective techniques, learn from each other, develop positive working relationships, and make their expeditions more successful, even if they have limited time to train together beforehand. This model can also inform the preparation and execution of actual future space flights. Published by Elsevier Ltd. on behalf of IAA.
C1 [Love, Stanley G.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Bleacher, Jacob E.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Love, SG (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM stanley.g.love@nasa.gov; jacob.e.bleacher@nasa.gov
RI Bleacher, Jacob/D-1051-2012
OI Bleacher, Jacob/0000-0002-8499-4828
FU Astronaut Office at Johnson Space Center; NASA Moon And Mars Analog
Mission Activities Program
FX The authors would like to thank the NASA Desert RATS team for providing
the opportunity to work together in the field. We also thank Aileen
Yingst and Janet Kavandi for helpful feedback on the content and
presentation of an early version of this paper. Reviewer Stephen
Robinson supplied many detailed and valuable suggestions directly to the
authors, in addition to his formal review. Two unnamed reviewers
provided further insightful comments. Stan Love's expenses for this work
were funded by the Astronaut Office at Johnson Space Center. Jake
Bleacher's support for the field test was provided by the Goddard Space
Flight Center's Solar System Exploration Division; funding for work
supporting Desert RATS and manuscript preparation was provided by a
grant from the NASA Moon And Mars Analog Mission Activities Program.
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SN 0094-5765
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JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 318
EP 331
DI 10.1016/j.actaastro.2011.12.012
PG 14
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100012
ER
PT J
AU Young, K
Hurtado, JM
Bleacher, JE
Garry, WB
Bleisath, S
Buffington, J
Rice, JW
AF Young, Kelsey
Hurtado, Jose M., Jr.
Bleacher, Jacob E.
Garry, W. Brent
Bleisath, Scott
Buffington, Jesse
Rice, James W., Jr.
TI Tools and technologies needed for conducting planetary field geology
while on EVA: Insights from the 2010 Desert RATS geologist crewmembers
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Field geology; Sample collection; Planetary analog; EVA technology; EVA
tools; Planetary field geology
AB The tools used by crews while on extravehicular activity during future missions to other bodies in the Solar System will be a combination of traditional geologic field tools (e.g. hammers, rakes, sample bags) and state-of-the-art technologies (e.g. high definition cameras, digital situational awareness devices, and new geologic tools). In the 2010 Desert Research and Technology Studies (RATS) field test, four crews, each consisting of an astronaut/engineer and field geologist, tested and evaluated various technologies during two weeks of simulated spacewalks in the San Francisco volcanic field, Arizona. These tools consisted of both Apollo-style field geology tools and modern technological equipment not used during the six Apollo lunar landings. The underlying exploration driver for this field test was to establish the protocols and technology needed for an eventual manned mission to an asteroid, the Moon, or Mars. The authors of this paper represent Desert RATS geologist crewmembers as well as two engineers who worked on technology development. Here we present an evaluation and assessment of these tools and technologies based on our first-hand experience of using them during the analog field test. We intend this to serve as a basis for continued development of technologies and protocols used for conducting planetary field geology as the Solar System exploration community moves forward into the next generation of planetary surface exploration. (C) 2011 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Young, Kelsey] Arizona State Univ, Sch Earth & Space Explorat, Bateman Phys Sci Ctr F Wing, Tempe, AZ 85287 USA.
[Hurtado, Jose M., Jr.] Univ Texas El Paso, Dept Geol Sci, El Paso, TX 79968 USA.
[Bleacher, Jacob E.; Rice, James W., Jr.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Garry, W. Brent] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Bleisath, Scott] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Buffington, Jesse] NASA, EVA Hardware Dev Tools & Equipment Branch EC7, Johnson Space Ctr, Houston, TX 77058 USA.
RP Young, K (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Bateman Phys Sci Ctr F Wing, Room 686, Tempe, AZ 85287 USA.
EM Kelsey.E.Young@asu.edu
RI Bleacher, Jacob/D-1051-2012; Garry, Brent/I-5920-2013
OI Bleacher, Jacob/0000-0002-8499-4828;
FU Constellation Program; NASA Graduate Student Researchers Program
[NNX10AK72H]; NASA [NNX10AK72H]; NASA Field Science Analog Testing
grant; NASA Minority Research and Education Program [NNX09AV09A]; NASA
Lunar Science Institute [NNA09DB33A]; NASA Lunar Science Institute
(LPI/USRA) [02173-07]; NASA Moon And Mars Analog Mission Activities
Program
FX The authors, especially those of us who served as 2010 geologist
crewmembers (Young, Bleacher, Hurtado, and Rice) would like to recognize
the large Desert RATS team that helped to make our experience such a
positive one. In particular, the incredibly gifted and extensive Science
Team working with us both prior to the test and back "on Earth" during
our missions was a crucial part in our success. Specifically, Cindy
Evans, Fred Horz, Gary Lofgren, John Gruener, Doug Ming, Mary Sue Bell,
Kip Hodges, and above all Dean Eppler, we thank you. We also wish to
thank our NASA astronaut and engineering crewmates without whom we would
not have been able to complete such a successful mission: Stephanie
Wilson, Stan Love, Mike Gernhardt, Chris Looper, and Aaron Hulse. Many
thanks go to the many funding organizations that made this work
possible. Acknowledgements go to Dr. Wendell Mendell, whose funding from
the Constellation Program enabled the assembly of the world-class
science team for this exercise. K. Young recognizes funding from the
NASA Graduate Student Researchers Program Grant #NNX10AK72H. J. Hurtado
acknowledges funding from a 2009 NASA Field Science Analog Testing
grant, NASA Minority Research and Education Program collaborative
agreement #NNX09AV09A, and NASA Lunar Science Institute cooperative
agreement #NNA09DB33A (LPI/USRA subcontract #02173-07), which supported
his participation in the 2009 and 2010 field tests. The Goddard Space
Flight Center's Solar System Exploration Division provided J. Bleacher
and J. Rice's support for the field test. J. Bleacher's Desert RATS
supporting work and manuscript preparation funding were provided by a
NASA Moon And Mars Analog Mission Activities Program grant. J.
Buffington's support for the field test was provided by the NASA Desert
RATS project and the Space Exploration Vehicle project.
NR 12
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SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 332
EP 343
DI 10.1016/j.actaastro.2011.10.016
PG 12
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100013
ER
PT J
AU Hurtado, JM
Young, K
Bleacher, JE
Garry, WB
Rice, JW
AF Hurtado, Jose M., Jr.
Young, Kelsey
Bleacher, Jacob E.
Garry, W. Brent
Rice, James W., Jr.
TI Field geologic observation and sample collection strategies for
planetary surface exploration: Insights from the 2010 Desert RATS
geologist crewmembers
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Field geology; Planetary analog; Sample collection; Field geology
methods; Extravehicular activity (EVA); Planetary field geology
AB Observation is the primary role of all field geologists, and geologic observations put into an evolving conceptual context will be the most important data stream that will be relayed to Earth during a planetary exploration mission. Sample collection is also an important planetary field activity, and its success is closely tied to the quality of contextual observations. To test protocols for doing effective planetary geologic fieldwork, the Desert RATS (Research and Technology Studies) project deployed two prototype rovers for two weeks of simulated exploratory traverses in the San Francisco volcanic field of northern Arizona: The authors of this paper represent the geologist crewmembers who participated in the 2010 field test. We document the procedures adopted for Desert RATS 2010 and report on our experiences regarding these protocols. Careful consideration must be made of various issues that impact the interplay between field geologic observations and sample collection, including time management; strategies related to duplication of samples and observations; logistical constraints on the volume and mass of samples and the volume/transfer of data collected; and paradigms for evaluation of mission success. We find that the 2010 field protocols brought to light important aspects of each of these issues, and we recommend best practices and modifications to training and operational protocols to address them. Underlying our recommendations is the recognition that the capacity of the crew to "flexibly execute" their activities is paramount. Careful design of mission parameters, especially field geologic protocols, is critical for enabling the crews to successfully meet their science objectives. (C) 2011 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Hurtado, Jose M., Jr.] Univ Texas El Paso, Dept Geol Sci, El Paso, TX 79968 USA.
[Young, Kelsey] Arizona State Univ, Sch Earth & Space Explorat, Bateman Phys Sci Ctr, Tempe, AZ 85287 USA.
[Bleacher, Jacob E.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Garry, W. Brent] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Rice, James W., Jr.] NASA, Solar Syst Explorat Div, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Hurtado, JM (reprint author), Univ Texas El Paso, Dept Geol Sci, 500 West Univ Ave, El Paso, TX 79968 USA.
EM jhurtado@utep.edu
RI Bleacher, Jacob/D-1051-2012; Garry, Brent/I-5920-2013
OI Bleacher, Jacob/0000-0002-8499-4828;
FU NASA Field Science Analog Testing grant; NASA Minority Research and
Education Program [NNX09AV09A]; NASA Lunar Science Institute
[NNA09DB33A]; NASA Lunar Science Institute (LPI/USRA) [02173-07]; NASA
Graduate Student Researchers Program [NNX10AK72H]; NASA Moon and Mars
Analog Mission Activities Program grant
FX The authors, all crewmembers for Desert RATS 2009 and/or 2010, send a
heartfelt thanks to all those individuals - in both Engineering and
Science and at all the NASA centers and a host of universities - who
have contributed their tireless work and immense talents to making
Desert RATS a success. Without your efforts, none of this would be
possible. Dr. Wendell Mendell provided funding from the Constellation
Program that enabled the assembly of the world-class science team for
Desert RATS. J. Hurtado acknowledges funding from a 2009 NASA Field
Science Analog Testing grant, NASA Minority Research and Education
Program collaborative agreement #NNX09AV09A, and NASA Lunar Science
Institute cooperative agreement #NNA09DB33A (LPI/USRA subcontract
#02173-07), which supported his participation in the 2009 and 2010 field
tests. K. Young recognizes funding from the NASA Graduate Student
Researchers Program Grant #NNX10AK72H. The Goddard Space Flight Center's
Solar System Exploration Division provided J. Bleacher's and J. Rice's
support for the field-test. Desert RATS supporting work and manuscript
preparation funding were provided by a NASA Moon and Mars Analog Mission
Activities Program grant. The authors also acknowledge the suggestions
of two anonymous reviewers whose input strengthened the manuscript.
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JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 344
EP 355
DI 10.1016/j.actaastro.2011.10.015
PG 12
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100014
ER
PT J
AU Bleacher, JE
Hurtado, JM
Young, KE
Rice, JW
Garry, WB
AF Bleacher, Jacob E.
Hurtado, Jose M., Jr.
Young, Kelsey E.
Rice, James W., Jr.
Garry, W. Brent
TI The effect of different operations modes on science capabilities during
the 2010 Desert RATS test: Insights from the geologist crewmembers
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Planetary geology; Field geology; Analogs; Human spaceflight;
Communications
AB The 2010 Desert RATS field test utilized two Space Exploration Vehicles (prototype planetary rovers) and four crewmembers (2 per rover) to conduct a geologic traverse across northern Arizona while testing continuous and twice-per-day communications paired with operation modes of separating and exploring individually (Divide & Conquer) and exploring together (Lead & Follow), respectively. This report provides qualitative conclusions from the geologist crewmembers involved in this test as to how these modes of communications and operations affected our ability to conduct field geology. Each mode of communication and operation provided beneficial capabilities that might be further explored for future Human Spaceflight Missions to other solar system objects. We find that more frequent interactions between crews and an Apollo-style Science Team on the Earth best enables scientific progress during human exploration. However, during multiple vehicle missions, this communication with an Earth-based team of scientists, who represent "more minds on the problem", should not come at the exclusion of (or significantly decrease) communication between the crewmembers in different vehicles who have the "eyes on the ground". Inter-crew communications improved when discussions with a backroom were infrequent. Both aspects are critical and cannot be mutually exclusive. Increased vehicle separation distances best enable encounters with multiple geologic units. However, seemingly redundant visits by multiple vehicles to the same feature can be utilized to provide improved process-related observations about the development and modification of the local terrain. We consider the value of data management, transfer, and accessibility to be the most important lesson learned. Crews and backrooms should have access to all data and related interpretations within the mission in as close to real-time conditions as possible. This ensures that while on another planetary surface, crewmembers are as educated as possible with respect to the observations and data they will need to collect at any moment. Published by Elsevier Ltd. on behalf of IAA.
C1 [Bleacher, Jacob E.; Rice, James W., Jr.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hurtado, Jose M., Jr.] Univ Texas El Paso, Dept Geol Sci, El Paso, TX 79968 USA.
[Young, Kelsey E.] Arizona State Univ, Sch Earth & Space Explorat, Bateman Phys Sci Ctr, Tempe, AZ 85287 USA.
[Garry, W. Brent] Planetary Sci Inst, Tucson, AZ 85719 USA.
RP Bleacher, JE (reprint author), NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Code 698,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM jacob.e.bleacher@nasa.gov
RI Bleacher, Jacob/D-1051-2012; Garry, Brent/I-5920-2013
OI Bleacher, Jacob/0000-0002-8499-4828;
FU NASA [NNX09AV09A, NNX10AK72H]; NASA Lunar Science Institute
[NNA09DB33A]; NASA Lunar Science Institute (LPI/USRA) [02173-07]
FX The Goddard Space Flight Center's Solar System Exploration Division
provided J. Bleacher and J. Rice's support for the field test. J.
Bleacher's Desert RATS supporting work and manuscript preparation
funding were provided by NASA's Moon And Mars Analog Mission Activities
Program. J. Hurtado acknowledges funding from a 2009 NASA Field Science
Analog Testing Grant, NASA Minority Research and Education Program
collaborative agreement #NNX09AV09A, and NASA Lunar Science Institute
cooperative agreement #NNA09DB33A (LPI/USRA subcontract #02173-07) which
supported his participation in the 2009 and 2010 field tests. K. Young
recognizes funding from the NASA Graduate Student Researchers Program
Grant #NNX10AK72H.
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PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 356
EP 366
DI 10.1016/j.actaastro.2011.10.018
PG 11
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100015
ER
PT J
AU Litaker, HL
Howard, RL
AF Litaker, Harry L., Jr.
Howard, Robert L., Jr.
TI Social network analysis and dual rover communications
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Social network analysis; Communications; Human factors; DRATS; Space
exploration vehicle
ID OPERATIONS
AB Social network analysis (SNA) refers to the collection of techniques, tools, and methods used in sociometry aiming at the analysis of social networks to investigate decision making, group communication, and the distribution of information. Human factors engineers at the National Aeronautics and Space Administration (NASA) conducted a social network analysis on communication data collected during a 14-day field study operating a dual rover exploration mission to better understand the relationships between certain network groups such as ground control, flight teams, and planetary science. The analysis identified two communication network structures for the continuous communication and Twice-a-Day Communication scenarios as a split network and negotiated network respectfully. The major nodes or groups for the networks' architecture, transmittal status, and information were identified using graphical network mapping, quantitative analysis of subjective impressions, and quantified statistical analysis using Sociometric Statue and Centrality. Post-questionnaire analysis along with interviews revealed advantages and disadvantages of each network structure with team members identifying the need for a more stable continuous communication network, improved robustness of voice loops, and better systems training/capabilities for scientific imagery data and operational data during Twice-a-Day Communications. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Litaker, Harry L., Jr.] Lockheed Martin, Houston, TX 77058 USA.
[Howard, Robert L., Jr.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Litaker, HL (reprint author), Lockheed Martin, 1300 Hercules,Mail Code C46, Houston, TX 77058 USA.
EM harry.l.litaker@nasa.gov
NR 18
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 367
EP 377
DI 10.1016/j.actaastro.2012.05.013
PG 11
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100016
ER
PT J
AU Litaker, HL
Thompson, SG
Szabo, R
Twyford, ES
Conlee, CS
Howard, RL
AF Litaker, Harry L., Jr.
Thompson, Shelby G.
Szabo, Richard
Twyford, Evan S.
Conlee, Carl S.
Howard, Robert L., Jr.
TI Dual rover human habitation field study
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Habitation; Space Exploration Vehicle; DRATS; Volume; Human factors
AB For the last 3 years, the National Aeronautics and Space Administration (NASA) has been testing a pressurized rover prototype in the deserts of Arizona to obtain humanin-the-loop performance data. This year's field trial consisted of operating two rovers simultaneously while embarking on two 7-day flight-like exploration missions. During the 2010 Desert Research and Technology Studies (DRATS) at Black Point Lava Flow and SP Mountain in Arizona, NASA human factors investigators, in cooperation with other engineers and scientists, collected data on both the daily living and working within and around the Space Exploration Vehicle (SEV). Both objective and subjective data were collected using standard human factors metrics. Over 305 h of crew habitability data were recorded during the field trial with 65 elements of habitation examined. Acceptability of the vehicles over the course of the missions was considered satisfactory by the majority of the crews. As with previous testing, habitation was considered acceptable by the crews, but some issues concerning stowage, Waste Containment System (WCS) volume, and sleep curtains need to be considered for redesign for the next generation vehicle. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Litaker, Harry L., Jr.; Thompson, Shelby G.; Szabo, Richard] Lockheed Martin, Houston, TX 77058 USA.
[Twyford, Evan S.; Conlee, Carl S.] MEI Technol, Houston, TX 77058 USA.
[Howard, Robert L., Jr.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Litaker, HL (reprint author), Lockheed Martin, 1300 Hercules,Mail Code C46, Houston, TX 77058 USA.
EM harry.l.litaker@nasa.gov
NR 7
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 378
EP 390
DI 10.1016/j.actaastro.2012.03.027
PG 13
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100017
ER
PT J
AU Litaker, HL
Archer, RD
Szabo, R
Twyford, ES
Conlee, CS
Howard, RL
AF Litaker, Harry L., Jr.
Archer, Ronald D.
Szabo, Richard
Twyford, Evan S.
Conlee, Carl S.
Howard, Robert L.
TI Human habitation field study of the Habitat Demonstration Unit (HDU)
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Habitation; Space Exploration Vehicle; Habitat Demonstration Unit; Human
factors; DRATS
AB Landing and supporting a permanent outpost on a planetary surface represents humankind's capability to expand its own horizons and challenge current technology. With this in mind, habitability of these structures becomes more essential given the longer durations of the missions. The purpose of this evaluation was to obtain preliminary human-in-the-loop performance data on the Habitat Demonstration Unit (HDU) in a Pressurized Excursion Module (PEM) configuration during a 14-day simulated lunar exploration field trial and to apply this knowledge to further enhance the habitat's capabilities for forward designs. Human factors engineers at the NASA/Johnson Space Center's Habitability and Human Factors Branch recorded approximately 96 h of crew task performance with four work stations. Human factors measures used during this study included the NASA Task Load Index (TLX) and customized post questionnaires. Overall the volume for the PEM was considered acceptable by the crew; however; the habitat's individual work station volume Was constrained when setting up the vehicle for operation, medical operations, and suit maintenance while general maintenance, logistical resupply, and geo science was considered acceptable. Crew workload for each station indicated resupply as being the lowest rated, with medical operations, general maintenance, and geo science tasks as being light, while suit maintenance was considered moderate and general vehicle setup being rated the highest. Stowage was an issue around the habitat with the Space Exploration Vehicle (SEV) resupply stowage located in the center of the habitat as interfering with some work station volumes and activities. Ergonomics of the geo science station was considered a major issue, especially with the overhead touch screens. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Litaker, Harry L., Jr.; Archer, Ronald D.; Szabo, Richard] Lockheed Martin, Houston, TX 77058 USA.
[Twyford, Evan S.; Conlee, Carl S.] MEI Technol, Houston, TX 77058 USA.
[Howard, Robert L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Litaker, HL (reprint author), Lockheed Martin, 1300 Hercules,Mail Code C46, Houston, TX 77058 USA.
EM harry.l.litaker@nasa.gov
NR 5
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 391
EP 405
DI 10.1016/j.actaastro.2012.04.018
PG 15
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100018
ER
PT J
AU Gruener, JE
Lofgren, GE
Bluethmann, WJ
Abercromby, AF
AF Gruener, J. E.
Lofgren, G. E.
Bluethmann, W. J.
Abercromby, A. F.
TI NASA Desert RATS 2010: Preliminary results for science operations
conducted in the San Francisco Volcanic Field, Arizona
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Desert RATS; Human spaceflight; Planetary exploration; San Francisco
volcanic field
AB The National Aeronautics and Space Administration (NASA) is working with international partners to develop the space architectures and mission plans necessary for human spaceflight beyond Earth orbit. The Apollo missions to the Moon demonstrated conclusively that surface mobility is a key asset that improves the efficiency of human explorers on a planetary surface. NASA's Desert Research and Technology Studies (Desert RATS), a multi-year series of tests of hardware and operations carried out annually in the high desert of Arizona, has tested a crewed pressurized rover concept referred to as the Space Exploration Vehicle (SEV). During NASA's Desert RATS 2010, four 2-person crews driving two SEVs collectively conducted 12 days of field exploration in the San Francisco Volcanic Field in northern Arizona. They collected 461 samples, with a total mass of 161.2 kg, on 70 simulated extravehicular activities (EVAs). Each SEV crew traveled over 60 km during their field explorations. This paper illustrates where the actual field sites, or 'science stations', were located, provides a brief description of the types of samples collected at each station, and highlights some of the more interesting sites. Most of the geologic samples collected at Desert RATS 2010 were well documented at the site of collection, and upon delivery to the Johnson Space Center the samples were given a preliminary examination. The samples are available for further study by interested researchers developing scientific instruments for use on the surfaces of the Moon and Mars, or for geological investigations of the San Francisco Volcanic Field. Published by Elsevier Ltd. on behalf of IAA.
C1 [Gruener, J. E.; Lofgren, G. E.; Bluethmann, W. J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Abercromby, A. F.] Wyle Integrated Sci & Engn, Houston, TX 77058 USA.
RP Gruener, JE (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM john.e.gruener@nasa.gov
NR 5
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT
PY 2013
VL 90
IS 2
SI SI
BP 406
EP 415
DI 10.1016/j.actaastro.2011.12.006
PG 10
WC Engineering, Aerospace
SC Engineering
GA 193LK
UT WOS:000322561100019
ER
PT J
AU Raj, SV
Noebe, RD
AF Raj, S. V.
Noebe, R. D.
TI Low temperature creep of hot-extruded near-stoichiometric NiTi shape
memory alloy part I: Isothermal creep
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
MICROSTRUCTURE AND PROCESSING
LA English
DT Article
DE Low temperature creep; NiTi; Shape memory alloys; Intermetallic alloys
ID NICKEL-TITANIUM ALLOYS; DEFORMATION TWINS; POWER-LAW; REORIENTATION;
BEHAVIOR; PHASE
AB This two-part paper is the first published report on the long term, low temperature creep of hot-extruded near-stoichiometric NiTi. Constant load tensile creep tests were conducted on hot-extruded near-stoichiometric NiTi at 300, 373 and 473 K under initial applied stresses varying between 200 and 350 MPa as long as 15 months. These temperatures corresponded to the martensitic, two-phase and austenitic phase regions, respectively. Normal primary creep lasting several months was observed under all conditions indicating dislocation activity. Although steady-state creep was not observed under these conditions, the estimated creep rates varied between 10(-10) and 10(-9) s(-1). The creep behavior of the two phases showed significant differences. The martensitic phase exhibited a large strain on loading followed by a primary creep region accumulating a small amount of strain over a period of several months. The loading strain was attributed to the detwinning of the martensitic phase whereas the subsequent strain accumulation was attributed to dislocation glide-controlled creep. An "incubation period" was observed before the occurrence of detwinning. In contrast, the austenitic phase exhibited a relatively smaller loading strain followed by a primary creep region, where the creep strain continued to increase over several months. It is concluded that the creep of the austenitic phase occurs by a dislocation glide-controlled creep mechanism as well as by the nucleation and growth of deformation twins. Published by Elsevier B.V.
C1 [Raj, S. V.; Noebe, R. D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Raj, SV (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
EM sai.v.raj@nasa.gov
FU Subsonic Fixed Wing Project of NASA's Fundamental Aeronautics Program
FX The authors thank Mr. Darrell Gaydosh, Drs. Anita Garg, Bradley Lerch
and Santo Padula for granting permission to cite or use their
unpublished data. The authors also thank Prof. R. D. James, University
of Minnesota, and Prof. P. Anderson, Ohio State University for
discussions relating to some of the data included in this paper.
Comments from Dr. Michael Nathal are greatly appreciated. This work was
supported by the Subsonic Fixed Wing Project of NASA's Fundamental
Aeronautics Program.
NR 35
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PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0921-5093
EI 1873-4936
J9 MAT SCI ENG A-STRUCT
JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process.
PD OCT 1
PY 2013
VL 581
BP 145
EP 153
DI 10.1016/j.msea.2013.04.040
PG 9
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 196UH
UT WOS:000322802400020
ER
PT J
AU Raj, SV
Noebe, RD
AF Raj, S. V.
Noebe, R. D.
TI Low temperature creep of hot-extruded near-stoichiometric NiTi shape
memory alloy part II: Effect of thermal cycling
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
MICROSTRUCTURE AND PROCESSING
LA English
DT Article
DE Low temperature creep; NiTi; Shape memory alloys; Thermo-mechanical
cycling
ID NICKEL-TITANIUM ALLOYS; DEFORMATION; TRANSFORMATION; MARTENSITE; PHASE
AB This paper is the first report on the effect prior low temperature creep on the thermal cycling behavior of NiTi. The isothermal low temperature creep behavior of near-stoichiometric NiTi between 300 and 473 K was discussed in part I. The effect of temperature cycling on its creep behavior is reported in the present paper (part II). Temperature cycling tests were conducted between either 300 or 373 K and 473 K under a constant applied stress of either 250 or 350 MPa with hold times lasting at each temperature varying between 300 and 700 h. Each specimen was pre-crept either at 300 or 473 K for several months under an identical applied stress as that used in the subsequent thermal cycling tests. Irrespective of the initial pre-crept microstructures, the specimens exhibited a considerable increase in strain with each thermal cycle so that the total strain continued to build-up to 15% to 20% after only 5 cycles. Creep strains were immeasurably small during the hold periods. It is demonstrated that the strains in the austenite and martensite are linearly correlated. Interestingly, the differential irrecoverable strain, Delta epsilon(irr), in the material measured in either phase decreases with increasing number of cycles, N, as Delta epsilon(irr)=4.3(N)(-0.5) similar to the well-known Manson-Coffin relation in low cycle fatigue. Both phases are shown to undergo strain hardening due to the development of residual stresses. Plots of true creep rate against absolute temperature showed distinct peaks and valleys during the cool-down and heat-up portions of the thermal cycles, respectively. Transformation temperatures determined from the creep data revealed that the austenitic start and finish temperatures were more sensitive to the pre-crept martensitic phase than to the pre-crept austenitic phase. The results are discussed in terms of a phenomenological model, where it is suggested that thermal cycling between the austenitic and martensitic phase temperatures or vice versa results in the deformation of the austenite and a corresponding development of a back stress due to a significant increase in the dislocation density during thermal cycling. Published by Elsevier B.V.
C1 [Raj, S. V.; Noebe, R. D.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Raj, SV (reprint author), NASA Glenn Res Ctr, MS 106-5,21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM sai.v.raj@nasa.gov
FU Subsonic Fixed Wing Project of NASA's Fundamental Aeronautics Program
FX This work was supported by the Subsonic Fixed Wing Project of NASA's
Fundamental Aeronautics Program.
NR 36
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U1 2
U2 37
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0921-5093
J9 MAT SCI ENG A-STRUCT
JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process.
PD OCT 1
PY 2013
VL 581
BP 154
EP 163
DI 10.1016/j.msea.2013.04.095
PG 10
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 196UH
UT WOS:000322802400021
ER
PT J
AU Yee, HC
Kotov, DV
Wang, W
Shu, CW
AF Yee, H. C.
Kotov, D. V.
Wang, Wei
Shu, Chi-Wang
TI Spurious behavior of shock-capturing methods by the fractional step
approach: Problems containing stiff source terms and discontinuities
(vol 241, pg 266. 2013)
SO JOURNAL OF COMPUTATIONAL PHYSICS
LA English
DT Correction
C1 [Yee, H. C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kotov, D. V.] Stanford Ctr Turbulence Res, Stanford, CA 94305 USA.
[Wang, Wei] Florida Int Univ, Dept Math & Stat, Miami, FL 33199 USA.
[Shu, Chi-Wang] Brown Univ, Div Appl Math, Providence, RI 02912 USA.
RP Yee, HC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Helen.M.Yee@nasa.gov
NR 1
TC 1
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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 0021-9991
J9 J COMPUT PHYS
JI J. Comput. Phys.
PD OCT 1
PY 2013
VL 250
BP 703
EP 712
DI 10.1016/j.jcp.2013.05.021
PG 10
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA 178GN
UT WOS:000321433800035
ER
PT J
AU Hanson, D
Hoover, S
Crites, A
Ade, PAR
Aird, KA
Austermann, JE
Beall, JA
Bender, AN
Benson, BA
Bleem, LE
Bock, JJ
Carlstrom, JE
Chang, CL
Chiang, HC
Cho, HM
Conley, A
Crawford, TM
de Haan, T
Dobbs, MA
Everett, W
Gallicchio, J
Gao, J
George, EM
Halverson, NW
Harrington, N
Henning, JW
Hilton, GC
Holder, GP
Holzapfel, WL
Hrubes, JD
Huang, N
Hubmayr, J
Irwin, KD
Keisler, R
Knox, L
Lee, AT
Leitch, E
Li, D
Liang, C
Luong-Van, D
Marsden, G
McMahon, JJ
Mehl, J
Meyer, SS
Mocanu, L
Montroy, TE
Natoli, T
Nibarger, JP
Novosad, V
Padin, S
Pryke, C
Reichardt, CL
Ruhl, JE
Saliwanchik, BR
Sayre, JT
Schaffer, KK
Schulz, B
Smecher, G
Stark, AA
Story, KT
Tucker, C
Vanderlinde, K
Vieira, JD
Viero, MP
Wang, G
Yefremenko, V
Zahn, O
Zemcov, M
AF Hanson, D.
Hoover, S.
Crites, A.
Ade, P. A. R.
Aird, K. A.
Austermann, J. E.
Beall, J. A.
Bender, A. N.
Benson, B. A.
Bleem, L. E.
Bock, J. J.
Carlstrom, J. E.
Chang, C. L.
Chiang, H. C.
Cho, H-M.
Conley, A.
Crawford, T. M.
de Haan, T.
Dobbs, M. A.
Everett, W.
Gallicchio, J.
Gao, J.
George, E. M.
Halverson, N. W.
Harrington, N.
Henning, J. W.
Hilton, G. C.
Holder, G. P.
Holzapfel, W. L.
Hrubes, J. D.
Huang, N.
Hubmayr, J.
Irwin, K. D.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E.
Li, D.
Liang, C.
Luong-Van, D.
Marsden, G.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mocanu, L.
Montroy, T. E.
Natoli, T.
Nibarger, J. P.
Novosad, V.
Padin, S.
Pryke, C.
Reichardt, C. L.
Ruhl, J. E.
Saliwanchik, B. R.
Sayre, J. T.
Schaffer, K. K.
Schulz, B.
Smecher, G.
Stark, A. A.
Story, K. T.
Tucker, C.
Vanderlinde, K.
Vieira, J. D.
Viero, M. P.
Wang, G.
Yefremenko, V.
Zahn, O.
Zemcov, M.
CA SPTpol Collaboration
TI Detection of B-Mode Polarization in the Cosmic Microwave Background with
Data from the South Pole Telescope
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID POWER SPECTRA; GRAVITY-WAVES; LIGHT; TEMPERATURE; CMB
AB Gravitational lensing of the cosmic microwave background generates a curl pattern in the observed polarization. This "B-mode" signal provides a measure of the projected mass distribution over the entire observable Universe and also acts as a contaminant for the measurement of primordial gravity-wave signals. In this Letter we present the first detection of gravitational lensing B modes, using first-season data from the polarization-sensitive receiver on the South Pole Telescope (SPTpol). We construct a template for the lensing B-mode signal by combining E-mode polarization measured by SPTpol with estimates of the lensing potential from a Herschel-SPIRE map of the cosmic infrared background. We compare this template to the B modes measured directly by SPTpol, finding a nonzero correlation at 7.7 sigma significance. The correlation has an amplitude and scale dependence consistent with theoretical expectations, is robust with respect to analysis choices, and constitutes the first measurement of a powerful cosmological observable.
C1 [Hanson, D.; Bender, A. N.; de Haan, T.; Dobbs, M. A.; Holder, G. P.; Smecher, G.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Hoover, S.; Crites, A.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Chiang, H. C.; Crawford, T. M.; Gallicchio, J.; Keisler, R.; Leitch, E.; Liang, C.; Luong-Van, D.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Schaffer, K. K.; Story, K. T.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Hoover, S.; Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Crites, A.; Carlstrom, J. E.; Crawford, T. M.; Leitch, E.; Liang, C.; Meyer, S. S.; Mocanu, L.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Ade, P. A. R.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3YB, S Glam, Wales.
[Aird, K. A.; Hrubes, J. D.] Univ Chicago, Chicago, IL 60637 USA.
[Austermann, J. E.; Cho, H-M.; Conley, A.; Everett, W.; Halverson, N. W.; Henning, J. W.] Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Beall, J. A.; Cho, H-M.; Gao, J.; Hilton, G. C.; Hubmayr, J.; Irwin, K. D.; Li, D.; Nibarger, J. P.] NIST, Boulder, CO 80305 USA.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K. T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Bock, J. J.; Padin, S.; Schulz, B.; Vieira, J. D.; Viero, M. P.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA.
[Bock, J. J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Carlstrom, J. E.; Chang, C. L.; Mehl, J.; Wang, G.; Yefremenko, V.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA.
[Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, ZA-4000 Durban, South Africa.
[George, E. M.; Harrington, N.; Holzapfel, W. L.; Huang, N.; Lee, A. T.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Novosad, V.; Yefremenko, V.] Argonne Natl Lab, Div Mat Sci, Argonne, IL 60439 USA.
[Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Schulz, B.] CALTECH, Ctr Infrared Proc & Anal, JPL, Pasadena, CA 91125 USA.
[Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
RP Hanson, D (reprint author), McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
RI Novosad, Valentyn/C-2018-2014; Holzapfel, William/I-4836-2015; Novosad,
V /J-4843-2015;
OI Aird, Kenneth/0000-0003-1441-9518; Reichardt,
Christian/0000-0003-2226-9169
FU National Science Foundation [ANT-0638937]; NSF [PHY-1125897, 0959620,
AST-0956135]; Gordon and Betty Moore Foundation [GBMF 947]; Office of
Science of the U.S. Department of Energy [DE-AC02-05CH11231,
DE-AC02-06CH11357]; National Sciences and Engineering Research Council
of Canada; Canada Research Chairs Program; Canadian Institute for
Advanced Research; Lorne Trottier Chair program in Astrophysics and
Cosmology at McGill; CITA National Fellowship program; NASA Hubble
Fellowship [HF-51275]
FX The SPT is supported by the National Science Foundation through Grant
No. ANT-0638937, with partial support provided by NSF Grant No.
PHY-1125897. Support for the development and construction of SPTpol were
provided by the Gordon and Betty Moore Foundation through Grant No. GBMF
947 to the University of Chicago, a gift from the Kavli Foundation, and
NSF Grant No. 0959620. Herschel is an ESA space observatory with science
instruments provided by European-led Principal Investigator consortia
and with important participation from NASA. This research used resources
of the National Energy Research Scientific Computing Center, which is
supported by the Office of Science of the U.S. Department of Energy
under Award No. DE-AC02-05CH11231. It also used resources of the CLUMEQ
supercomputing consortium, part of the Compute Canada network. Research
at Argonne National Laboratory and use of the Center for Nanoscale
Materials are supported by the Office of Science of the U.S. Department
of Energy under Award No. DE-AC02-06CH11357. The McGill group
acknowledges funding from the National Sciences and Engineering Research
Council of Canada, Canada Research Chairs Program, and the Canadian
Institute for Advanced Research. The C. U. Boulder group acknowledges
support from NSF Grant No. AST-0956135. We thank P. Hargrave at Cardiff
University for antireflection coating the SPTpol lens, A. Datesman for
his work on TES detectors at Argonne, R. Divan for microfabrication
support at Argonne, and the members of the Truce Collaboration for their
efforts in the design of the 150 GHz polarization detectors, in
particular D. Becker, J. Britton, M. D. Niemack, and K. W. Yoon at NIST.
We thank M. Lueker, T. Plagge, Z. Staniszewski, E. Shirokoff, H.
Spieler, and R. Williamson for their considerable contributions to the
SPT program. D. H. was supported by the Lorne Trottier Chair program in
Astrophysics and Cosmology at McGill and by the CITA National Fellowship
program. R. K. acknowledges support from NASA Hubble Fellowship Grant
No. HF-51275.
NR 50
TC 148
Z9 148
U1 2
U2 20
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 SEP 30
PY 2013
VL 111
IS 14
AR 141301
DI 10.1103/PhysRevLett.111.141301
PG 6
WC Physics, Multidisciplinary
SC Physics
GA 230TO
UT WOS:000325366100001
PM 24138230
ER
PT J
AU Coats, S
Smerdon, JE
Cook, BI
Seager, R
AF Coats, Sloan
Smerdon, Jason E.
Cook, Benjamin I.
Seager, Richard
TI Stationarity of the tropical pacific teleconnection to North America in
CMIP5/PMIP3 model simulations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ENSO; global climate models; climate change and variability;
climatology; North America; teleconnection
ID UNITED-STATES; SST ANOMALIES; ENSO; VARIABILITY; CLIMATE; PRECIPITATION;
DROUGHT; 20TH-CENTURY; MECHANISMS; MILLENNIUM
AB The temporal stationarity of the teleconnection between the tropical Pacific Ocean and North America (NA) is analyzed in atmosphere-only, and coupled last-millennium, historical, and control runs from the Coupled Model Intercomparison Project Phase 5 data archive. The teleconnection, defined as the correlation between December-January-February (DJF) tropical Pacific sea surface temperatures (SSTs) and DJF 200 mb geopotential height, is found to be nonstationary on multidecadal timescales. There are significant changes in the spatial features of the teleconnection over NA in continuous 56-year segments of the last millennium and control simulations. Analysis of atmosphere-only simulations forced with observed SSTs indicates that atmospheric noise cannot account for the temporal variability of the teleconnection, which instead is likely explained by the strength of, and multidecadal changes in, tropical Pacific Ocean variability. These results have implications for teleconnection-based analyses of model fidelity in simulating precipitation, as well as any reconstruction and forecasting efforts that assume stationarity of the observed teleconnection.
C1 [Coats, Sloan; Smerdon, Jason E.; Seager, Richard] Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Coats, S (reprint author), Lamont Doherty Earth Observ, 103B Oceanog,61 Route 9W POB 1000, Palisades, NY 10964 USA.
EM sjc2164@columbia.edu
RI Smerdon, Jason/F-9952-2011; Cook, Benjamin/H-2265-2012
FU NOAA [NA10OAR4310137]; NSF [ATM09-02716]
FX This work was supported by NOAA award NA10OAR4310137 (Global Decadal
Hydroclimate Variability and Change, GloDecH) and NSF award ATM09-02716.
We acknowledge the World Climate Research Programme's Working Group on
Coupled Modelling, which is responsible for CMIP, and we thank the
climate modeling groups (listed in Table S1) for producing and making
available their model output. For CMIP, the U.S. 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 LDEO contribution 7723.
NR 34
TC 22
Z9 22
U1 1
U2 16
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 SEP 28
PY 2013
VL 40
IS 18
BP 4927
EP 4932
DI 10.1002/grl.50938
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 233IU
UT WOS:000325562600026
ER
PT J
AU Worden, J
Jiang, Z
Jones, DBA
Alvarado, M
Bowman, K
Frankenberg, C
Kort, EA
Kulawik, SS
Lee, M
Liu, JJ
Payne, V
Wecht, K
Worden, H
AF Worden, John
Jiang, Zhe
Jones, Dylan B. A.
Alvarado, Matthew
Bowman, Kevin
Frankenberg, Christian
Kort, Eric A.
Kulawik, Susan S.
Lee, Meemong
Liu, Junjie
Payne, Vivienne
Wecht, Kevin
Worden, Helen
TI El Nino, the 2006 Indonesian peat fires, and the distribution of
atmospheric methane
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE methane; fires; ENSO; remote sensing
ID GEOS-CHEM; CO; EMISSIONS; TES; CH4; VARIABILITY; RESOLUTION; TRANSPORT;
MOPITT
AB Dry conditions from a moderate El Nino during the fall of 2006 resulted in enhanced burning in Indonesia with fire emissions of CO approximately 4-6 times larger than the prior year. Here we use new tropospheric methane and CO data from the Aura Tropospheric Emission Spectrometer and new CO profile measurements from the Terra Measurements of Pollution in the Troposphere (MOPITT) satellite instruments with the Goddard Earth Observing System (GEOS)-Chem model to estimate methane emissions of 4.25 0.75 Tg for October-November 2006 from these fires. Errors in convective parameterization in GEOS-Chem, evaluated by comparing MOPITT and GEOS-Chem CO profiles, are the primary uncertainty of the emissions estimate. The El Nino related Indonesian fires increased the tropical distribution of atmospheric methane relative to 2005, indicating that tropical biomass burning can compensate for expected decreases in tropical wetland methane emissions from reduced rainfall during El Nino as found in previous studies.
C1 [Worden, John; Jiang, Zhe; Bowman, Kevin; Frankenberg, Christian; Kort, Eric A.; Kulawik, Susan S.; Lee, Meemong; Liu, Junjie; Payne, Vivienne] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jiang, Zhe; Jones, Dylan B. A.] Univ Toronto, Toronto, ON, Canada.
[Alvarado, Matthew] Atmospher & Environm Res Inc, Lexington, MA USA.
[Kort, Eric A.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Wecht, Kevin] Harvard Univ, Cambridge, MA 02138 USA.
[Worden, Helen] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Worden, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 233-202G, Pasadena, CA 91109 USA.
EM john.r.worden@jpl.nasa.gov
RI Kort, Eric/F-9942-2012; Frankenberg, Christian/A-2944-2013; Chem,
GEOS/C-5595-2014; Jones, Dylan/O-2475-2014
OI Kort, Eric/0000-0003-4940-7541; Frankenberg,
Christian/0000-0002-0546-5857; Jones, Dylan/0000-0002-1935-3725
FU National Aeronautics and Space Administration; Natural Sciences and
Engineering Research Council of Canada; National Aeronautics and Space
Administration (NASA) Earth Observing System (EOS) Program; National
Science Foundation
FX 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. Work at the University of Toronto
was carried out with support from the Natural Sciences and Engineering
Research Council of Canada. The Mauna Loa data in figure was provided by
the NOAA ESRL website. The NCAR MOPITT project is supported by the
National Aeronautics and Space Administration (NASA) Earth Observing
System (EOS) Program. The National Center for Atmospheric Research
(NCAR) is sponsored by the National Science Foundation.
NR 21
TC 15
Z9 15
U1 1
U2 29
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 SEP 28
PY 2013
VL 40
IS 18
BP 4938
EP 4943
DI 10.1002/grl.50937
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 233IU
UT WOS:000325562600028
ER
PT J
AU Shen, BW
DeMaria, M
Li, JLF
Cheung, S
AF Shen, B. -W.
DeMaria, M.
Li, J. -L. F.
Cheung, S.
TI Genesis of Hurricane Sandy (2012) simulated with a global mesoscale
model
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Hurricane Sandy; genesis predictability; global mesoscale model; MJO;
multiscale interactions; easterly wave
ID TROPICAL CYCLOGENESIS; PREDICTABILITY; PACIFIC; FLOW
AB In this study, we investigate the formation predictability of Hurricane Sandy (2012) with a global mesoscale model. We first present five track and intensity forecasts of Sandy initialized at 00Z 22-26 October 2012, realistically producing its movement with a northwestward turn prior to its landfall. We then show that three experiments initialized at 00Z 16-18 October captured the genesis of Sandy with a lead time of up to 6days and simulated reasonable evolution of Sandy's track and intensity in the next 2day period of 18Z 21-23 October. Results suggest that the extended lead time of formation prediction is achieved by realistic simulations of multiscale processes, including (1) the interaction between an easterly wave and a low-level westerly wind belt (WWB) and (2) the appearance of the upper-level trough at 200hPa to Sandy's northwest. The low-level WWB and upper-level trough are likely associated with a Madden-Julian Oscillation.
C1 [Shen, B. -W.] UMCP ESSIC, College Pk, MD USA.
[Shen, B. -W.] NASA GSFC, Greenbelt, MD USA.
[DeMaria, M.] NOAA NESDIS, Ft Collins, CO USA.
[Li, J. -L. F.] CalTech JPL, Pasadena, CA USA.
[Cheung, S.] NASA ARC, Moffett Field, CA USA.
RP Shen, BW (reprint author), Univ Maryland, ESSIC, 5825 Univ Res Ct 4001, College Pk, MD 20740 USA.
EM bo-wen.shen-1@nasa.gov
RI DeMaria, Mark/F-5583-2010
FU NASA ESTO Advanced Information Systems Technology (AIST) program; NASA
Computational Modeling Algorithms and Cyberinfrastructure (CMAC) program
FX We are grateful for support from the NASA ESTO Advanced Information
Systems Technology (AIST) program and NASA Computational Modeling
Algorithms and Cyberinfrastructure (CMAC) program. We would also like to
thank reviewers for valuable comments, D. Ellsworth for scientific,
insightful visualizations, and K. Massaro, J. Pillard, and J. Dunbar for
proofreading this manuscript. Acknowledgment is also made to the NASA
HEC Program, the NAS Division, and the NCCS for the computer resources
used in this research. The views, opinions, and findings contained in
this report are those of the authors and should not be construed as an
official NOAA or U.S. government position, policy, or decision.
NR 20
TC 8
Z9 8
U1 1
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 SEP 28
PY 2013
VL 40
IS 18
BP 4944
EP 4950
DI 10.1002/grl.50934
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 233IU
UT WOS:000325562600029
ER
PT J
AU Yang, K
Dickerson, RR
Carn, SA
Ge, C
Wang, J
AF Yang, Kai
Dickerson, Russell R.
Carn, Simon A.
Ge, Cui
Wang, Jun
TI First observations of SO2 from the satellite Suomi NPP OMPS: Widespread
air pollution events over China
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE air pollution; sulfur dioxide; smog; SNPP; OMPS; UV retrieval
ID OZONE MONITORING INSTRUMENT; SCIAMACHY; RETRIEVAL; GOME
AB Severe smog episodes over China in January 2013 received worldwide attention. This air pollution was distinguished by heavy loadings of fine particulate matter and SO2. To characterize these episodes, we employed the Ozone Mapping and Profiler Suite, Nadir Mapper (OMPS NM), an ultraviolet (UV) spectrometer flying on the Suomi National Polar-orbiting Partnership (SNPP) spacecraft since October 2011. We developed an advanced algorithm to quantify SO2 in the lower troposphere and achieved high-quality retrievals from OMPS NM, which are characterized by high precision, approximate to 0.2 Dobson Units (DU; 1 DU = 2.69x10(16)molecules/cm(2)) for instantaneous field of view SO2 data and low biases (within 0.2 DU). Here we report SO(2)retrievals and UV aerosol index data for these pollution events. The SO2 columns and the areas covered by high pollutant concentrations are quantified; the results reveal for the first time the full extent (an area of approximate to 10(6)km(2) containing up to 60 kt of SO2) of these episodes.
C1 [Yang, Kai; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Yang, Kai] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
[Carn, Simon A.] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA.
[Ge, Cui; Wang, Jun] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA.
RP Yang, K (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Code 614,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Kai.Yang-1@nasa.gov
RI Wang, Jun/A-2977-2008; Dickerson, Russell/F-2857-2010; Ge,
Cui/I-6353-2016
OI Wang, Jun/0000-0002-7334-0490; Dickerson, Russell/0000-0003-0206-3083;
Ge, Cui/0000-0002-6182-6856
FU NASA [NNX11AK95G]
FX This work is supported by NASA under grant NNX11AK95G (Continuation of
Long-Term Sulfur Dioxide EDR with the SNPP/OMPS NM). We acknowledge the
use of OMPS Level 1B data produced by the SNPP Ozone Product Evaluation
and Algorithm Test Element (PEATE), funded by NASA. The authors thank
the editor and the two anonymous reviewers for their suggestions and
constructive comments.
NR 29
TC 26
Z9 28
U1 1
U2 24
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 SEP 28
PY 2013
VL 40
IS 18
BP 4957
EP 4962
DI 10.1002/grl.50952
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 233IU
UT WOS:000325562600031
ER
PT J
AU Kundu, PK
Travis, JE
AF Kundu, Prasun K.
Travis, James E.
TI A stochastic fractional dynamics model of space-time variability of rain
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GAUGE MEASUREMENTS; GROUND VALIDATION; MEASURING MISSION;
SIMPLEX-METHOD; STATISTICS
C1 [Kundu, Prasun K.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Kundu, Prasun K.] NASA, Goddard Space Flight Ctr, Joint Ctr Earth Syst Technol, Greenbelt, MD 20771 USA.
[Travis, James E.] Univ Maryland Baltimore Cty, Dept Math & Stat, Baltimore, MD 21228 USA.
RP Kundu, PK (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, 5523 Res Pk Dr, Baltimore, MD 21228 USA.
EM prasun.k.kundu@nasa.gov
FU GPM (Global Precipitation Measurement) GV group as a part of the NASA
Precipitation Measurement Missions (PMM) program; JCET Fellowship
FX We thank David Marks of Science Systems Applications International, Inc.
and NASA/GSFC for in-depth discussions on various details regarding the
TRMM GV data used in this study and for providing us with Figure 1. We
are also grateful to Bikas K. Sinha of Department of Mathematics and
Statistics, UMBC for his careful reading of the paper and Anindya Roy
also of Department of Mathematics and Statistics, UMBC for many helpful
discussions. Comments and constructive criticisms from the associate
editor and two other anonymous reviewers on various aspects of the work,
especially the parameter estimation method, greatly helped to improve
the presentation of the paper. The research conducted in this paper was
supported by the GPM (Global Precipitation Measurement) GV group as a
part of the NASA Precipitation Measurement Missions (PMM) program. One
of us (J.E.T.) gratefully acknowledges financial support from a JCET
Fellowship.
NR 27
TC 2
Z9 2
U1 1
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 SEP 27
PY 2013
VL 118
IS 18
BP 10277
EP 10295
DI 10.1002/jgrd.50723
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 239LJ
UT WOS:000326025200004
ER
PT J
AU Wilson, RC
Hook, SJ
Schneider, P
Schladow, SG
AF Wilson, R. Chris
Hook, Simon J.
Schneider, Philipp
Schladow, S. Geoffrey
TI Skin and bulk temperature difference at Lake Tahoe: A case study on lake
skin effect
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; COOL-SKIN; OCEAN SKIN; VALIDATION; PACIFIC;
PROJECT
C1 [Wilson, R. Chris; Hook, Simon J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schneider, Philipp] NILU Norwegian Inst Air Res, Kjeller, Norway.
[Schladow, S. Geoffrey] Univ Calif Davis, UC Davis Tahoe Environm Res Ctr, Davis, CA 95616 USA.
[Schladow, S. Geoffrey] Univ Calif Davis, Dept Civil & Environm Engn, Davis, CA 95616 USA.
RP Wilson, RC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM r.chris.wilson@gmail.com
FU National Aeronautics and Space Administration; NASA award as part of the
NASA EOS program
FX We thank Brant Allen of the UC Davis Tahoe Environmental Research Center
for his efforts in physically maintaining the Lake Tahoe buoys. We also
thank Evan Fishbein for his editing assistance. 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. The work was funded by a NASA
award to Simon Hook as part of the NASA EOS program.
NR 30
TC 11
Z9 12
U1 1
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 SEP 27
PY 2013
VL 118
IS 18
BP 10332
EP 10346
DI 10.1002/jgrd.50786
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 239LJ
UT WOS:000326025200021
ER
PT J
AU Luo, M
Read, W
Kulawik, S
Worden, J
Livesey, N
Bowman, K
Herman, R
AF Luo, Ming
Read, William
Kulawik, Susan
Worden, John
Livesey, Nathaniel
Bowman, Kevin
Herman, Robert
TI Carbon monoxide (CO) vertical profiles derived from joined TES and MLS
measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MICROWAVE LIMB SOUNDER; AURA SATELLITE; FEBRUARY 2009; EOS MLS; MISSION;
PRODUCTS; MODEL; DISTRIBUTIONS; OBJECTIVES; SYSTEM
C1 [Luo, Ming; Read, William; Kulawik, Susan; Worden, John; Livesey, Nathaniel; Bowman, Kevin; Herman, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Luo, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Ming.Luo@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX We would like to thank the strong support from the Aura project, TES and
MLS teams. We thank the AirCore team for conducting the balloon flights
and providing the analyzed CO data to support this project. 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.
NR 40
TC 3
Z9 3
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 SEP 27
PY 2013
VL 118
IS 18
BP 10601
EP 10613
DI 10.1002/jgrd.50800
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 239LJ
UT WOS:000326025200003
ER
PT J
AU Gurnett, DA
Kurth, WS
Burlaga, LF
Ness, NF
AF Gurnett, D. A.
Kurth, W. S.
Burlaga, L. F.
Ness, N. F.
TI In Situ Observations of Interstellar Plasma with Voyager 1
SO SCIENCE
LA English
DT Article
ID WIND TERMINATION SHOCK; GALACTIC COSMIC-RAYS; SOLAR-WIND;
MAGNETIC-FIELDS; OUTER HELIOSPHERE; RADIO-EMISSION; HELIOSHEATH; REGION;
WAVE; INTENSITY
AB Launched over 35 years ago, Voyagers 1 and 2 are on an epic journey outward from the Sun to reach the boundary between the solar plasma and the much cooler interstellar medium. The boundary, called the heliopause, is expected to be marked by a large increase in plasma density, from about 0.002 per cubic centimeter (cm(-3)) in the outer heliosphere, to about 0.1 cm(-3) in the interstellar medium. On 9 April 2013, the Voyager 1 plasma wave instrument began detecting locally generated electron plasma oscillations at a frequency of about 2.6 kilohertz. This oscillation frequency corresponds to an electron density of about 0.08 cm(-3), very close to the value expected in the interstellar medium. These and other observations provide strong evidence that Voyager 1 has crossed the heliopause into the nearby interstellar plasma.
C1 [Gurnett, D. A.; Kurth, W. S.] Univ Iowa, Iowa City, IA 52242 USA.
[Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ness, N. F.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Gurnett, DA (reprint author), Univ Iowa, Iowa City, IA 52242 USA.
EM donald-gurnett@uiowa.edu
OI Kurth, William/0000-0002-5471-6202
FU NASA [1415150, NNG11PM48P, NNX12AC63G]; JPL
FX We thank E. C. Stone, S. M. Krimigis, and J. D. Richardson, for their
helpful comments. We also thank R. B. Decker, L. J. Granroth, J. C.
Hall, A. Persoon, O. Santolik, and R. F. Wong for help in various data
processing issues. The research at Iowa was supported by NASA through
contract 1415150 with the JPL. The research at GSFC was supported by
NASA contract NNG11PM48P, and the research at CUA was supported in part
by NASA grant NNX12AC63G.
NR 32
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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 SEP 27
PY 2013
VL 341
IS 6153
BP 1489
EP 1492
DI 10.1126/science.1241681
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 224NS
UT WOS:000324894600043
PM 24030496
ER
PT J
AU Bish, DL
Blake, DF
Vaniman, DT
Chipera, SJ
Morris, RV
Ming, DW
Treiman, AH
Sarrazin, P
Morrison, SM
Downs, RT
Achilles, CN
Yen, AS
Bristow, TF
Crisp, JA
Morookian, JM
Farmer, JD
Rampe, EB
Stolper, EM
Spanovich, N
AF Bish, D. L.
Blake, D. F.
Vaniman, D. T.
Chipera, S. J.
Morris, R. V.
Ming, D. W.
Treiman, A. H.
Sarrazin, P.
Morrison, S. M.
Downs, R. T.
Achilles, C. N.
Yen, A. S.
Bristow, T. F.
Crisp, J. A.
Morookian, J. M.
Farmer, J. D.
Rampe, E. B.
Stolper, E. M.
Spanovich, N.
CA MSL Sci Team
TI X-ray Diffraction Results from Mars Science Laboratory: Mineralogy of
Rocknest at Gale Crater
SO SCIENCE
LA English
DT Article
ID GUSEV CRATER; SPECTROMETER; CHEMISTRY; ROVER; DUST
AB The Mars Science Laboratory rover Curiosity scooped samples of soil from the Rocknest aeolian bedform in Gale crater. Analysis of the soil with the Chemistry and Mineralogy (CheMin) x-ray diffraction (XRD) instrument revealed plagioclase (similar to An57), forsteritic olivine (similar to Fo62), augite, and pigeonite, with minor K-feldspar, magnetite, quartz, anhydrite, hematite, and ilmenite. The minor phases are present at, or near, detection limits. The soil also contains 27 +/- 14 weight percent x-ray amorphous material, likely containing multiple Fe3+- and volatile-bearing phases, including possibly a substance resembling hisingerite. The crystalline component is similar to the normative mineralogy of certain basaltic rocks from Gusev crater on Mars and of martian basaltic meteorites. The amorphous component is similar to that found on Earth in places such as soils on the Mauna Kea volcano, Hawaii.
C1 [Bish, D. L.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
[Blake, D. F.; Bristow, T. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Vaniman, D. T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Chipera, S. J.] Chesapeake Energy, Oklahoma City, OK 73154 USA.
[Morris, R. V.; Ming, D. W.; Rampe, E. B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Treiman, A. H.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Sarrazin, P.] In Xitu, Campbell, CA 95008 USA.
[Morrison, S. M.; Downs, R. T.] Univ Arizona, Dept Geol, Tucson, AZ 85721 USA.
[Achilles, C. N.] United Technol Corp Aerosp Syst, Engn & Sci Contract Grp, Houston, TX 77058 USA.
[Yen, A. S.; Crisp, J. A.; Morookian, J. M.; Spanovich, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Farmer, J. D.] Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA.
[Stolper, E. M.] CALTECH, Pasadena, CA 91125 USA.
RP Bish, DL (reprint author), Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
EM bish@indiana.edu
RI Martin-Torres, Francisco Javier/G-6329-2015; Blanco, Juan
Jose/E-3627-2014; Crisp, Joy/H-8287-2016; Harri, Ari-Matti/C-7142-2012;
Glavin, Daniel/D-6194-2012; Zorzano, Maria-Paz/F-2184-2015; Dworkin,
Jason/C-9417-2012; szopa, cyril/C-6865-2015; Gonzalez,
Rafael/D-1748-2009; Lemmon, Mark/E-9983-2010; Balic-Zunic,
Tonci/A-6362-2013; de Pablo, Miguel Angel/J-6442-2014; Gomez-Elvira,
Javier/K-5829-2014; Ramos, Miguel/K-2230-2014; Gomez,
Felipe/L-7315-2014; Rodriguez-Manfredi, Jose/L-8001-2014; Hayes,
Alexander/P-2024-2014; Zorzano, Maria-Paz/C-5784-2015
OI Martin-Torres, Francisco Javier/0000-0001-6479-2236; Blanco, Juan
Jose/0000-0002-8666-0696; Crisp, Joy/0000-0002-3202-4416; Harri,
Ari-Matti/0000-0001-8541-2802; Glavin, Daniel/0000-0001-7779-7765;
Zorzano, Maria-Paz/0000-0002-4492-9650; Dworkin,
Jason/0000-0002-3961-8997; Muller, Jan-Peter/0000-0002-5077-3736; szopa,
cyril/0000-0002-0090-4056; Lemmon, Mark/0000-0002-4504-5136;
Balic-Zunic, Tonci/0000-0003-1687-1233; de Pablo, Miguel
Angel/0000-0002-4496-2741; Gomez-Elvira, Javier/0000-0002-9068-9846;
Ramos, Miguel/0000-0003-3648-6818; Gomez, Felipe/0000-0001-9977-7060;
Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Hayes,
Alexander/0000-0001-6397-2630; Zorzano, Maria-Paz/0000-0002-4492-9650
FU NASA Mars Science Laboratory Mission; National Aeronautics and Space
Administration
FX Support from the NASA Mars Science Laboratory Mission is gratefully
acknowledged. Some 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. XRD
data presented here are archived in the Planetary Data System (PDS,
pds.nasa.gov).
NR 31
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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 SEP 27
PY 2013
VL 341
IS 6153
AR 1238932
DI 10.1126/science.1238932
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 224NS
UT WOS:000324894600002
PM 24072925
ER
PT J
AU Blake, DF
Morris, RV
Kocurek, G
Morrison, SM
Downs, RT
Bish, D
Ming, DW
Edgett, KS
Rubin, D
Goetz, W
Madsen, MB
Sullivan, R
Gellert, R
Campbell, I
Treiman, AH
McLennan, SM
Yen, AS
Grotzinger, J
Vaniman, DT
Chipera, SJ
Achilles, CN
Rampe, EB
Sumner, D
Meslin, PY
Maurice, S
Forni, O
Gasnault, O
Fisk, M
Schmidt, M
Mahaffy, P
Leshin, LA
Glavin, D
Steele, A
Freissinet, C
Navarro-Gonzalez, R
Yingst, RA
Kah, LC
Bridges, N
Lewis, KW
Bristow, TF
Farmer, JD
Crisp, JA
Stolper, EM
Marais, DJD
Sarrazin, P
AF Blake, D. F.
Morris, R. V.
Kocurek, G.
Morrison, S. M.
Downs, R. T.
Bish, D.
Ming, D. W.
Edgett, K. S.
Rubin, D.
Goetz, W.
Madsen, M. B.
Sullivan, R.
Gellert, R.
Campbell, I.
Treiman, A. H.
McLennan, S. M.
Yen, A. S.
Grotzinger, J.
Vaniman, D. T.
Chipera, S. J.
Achilles, C. N.
Rampe, E. B.
Sumner, D.
Meslin, P-Y.
Maurice, S.
Forni, O.
Gasnault, O.
Fisk, M.
Schmidt, M.
Mahaffy, P.
Leshin, L. A.
Glavin, D.
Steele, A.
Freissinet, C.
Navarro-Gonzalez, R.
Yingst, R. A.
Kah, L. C.
Bridges, N.
Lewis, K. W.
Bristow, T. F.
Farmer, J. D.
Crisp, J. A.
Stolper, E. M.
Marais, D. J. Des
Sarrazin, P.
CA MSL Sci Team
TI Curiosity at Gale Crater, Mars: Characterization and Analysis of the
Rocknest Sand Shadow
SO SCIENCE
LA English
DT Article
ID MERIDIANI-PLANUM; LANDING SITE; SALTATION; DEPOSITS; DUNES
AB The Rocknest aeolian deposit is similar to aeolian features analyzed by the Mars Exploration Rovers (MERs) Spirit and Opportunity. The fraction of sand <150 micrometers in size contains similar to 55% crystalline material consistent with a basaltic heritage and similar to 45% x-ray amorphous material. The amorphous component of Rocknest is iron-rich and silicon-poor and is the host of the volatiles (water, oxygen, sulfur dioxide, carbon dioxide, and chlorine) detected by the Sample Analysis at Mars instrument and of the fine-grained nanophase oxide component first described from basaltic soils analyzed by MERs. The similarity between soils and aeolian materials analyzed at Gusev Crater, Meridiani Planum, and Gale Crater implies locally sourced, globally similar basaltic materials or globally and regionally sourced basaltic components deposited locally at all three locations.
C1 [Blake, D. F.; Bristow, T. F.; Marais, D. J. Des] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Morris, R. V.; Ming, D. W.; Achilles, C. N.; Rampe, E. B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Kocurek, G.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA.
[Morrison, S. M.; Downs, R. T.] Univ Arizona, Dept Geol, Tucson, AZ 85721 USA.
[Bish, D.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
[Edgett, K. S.] Malin Space Sci Syst, San Diego, CA 92191 USA.
[Rubin, D.] US Geol Survey, Santa Cruz, CA 95060 USA.
[Goetz, W.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Madsen, M. B.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Sullivan, R.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14850 USA.
[Gellert, R.; Campbell, I.] Univ Guelph, Guelph, ON N1G 2W1, Canada.
[Treiman, A. H.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[McLennan, S. M.] SUNY Stony Brook, Stony Brook, NY 11790 USA.
[Yen, A. S.; Crisp, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grotzinger, J.; Stolper, E. M.] CALTECH, Pasadena, CA 91125 USA.
[Vaniman, D. T.; Yingst, R. A.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Chipera, S. J.] Chesapeake Energy, Oklahoma City, OK 73102 USA.
[Sumner, D.] Univ Calif Davis, Davis, CA 95616 USA.
[Meslin, P-Y.; Maurice, S.; Forni, O.; Gasnault, O.] UPS OMP CNRS, IRAP, F-31028 Toulouse, France.
[Fisk, M.] Oregon State Univ, Corvallis, OR 97331 USA.
[Schmidt, M.] Finnish Meteorol Inst, FI-00101 Helsinki, Finland.
[Mahaffy, P.; Glavin, D.; Freissinet, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Leshin, L. A.] Rensselaer Polytech Inst, Troy, NY 12180 USA.
[Steele, A.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Navarro-Gonzalez, R.] Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico.
[Kah, L. C.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Bridges, N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Lewis, K. W.] Princeton Univ, Princeton, NJ 08544 USA.
[Farmer, J. D.] Arizona State Univ, Phoenix, AZ 85004 USA.
[Sarrazin, P.] SETI Inst, Mountain View, CA 94043 USA.
RP Blake, DF (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM david.blake@nasa.gov
RI Gomez-Elvira, Javier/K-5829-2014; Ramos, Miguel/K-2230-2014; Gomez,
Felipe/L-7315-2014; Rodriguez-Manfredi, Jose/L-8001-2014; Madsen,
Morten/D-2082-2011; Gonzalez, Rafael/D-1748-2009; Lemmon,
Mark/E-9983-2010; Glavin, Daniel/D-6194-2012; Frydenvang,
Jens/D-4781-2013; Balic-Zunic, Tonci/A-6362-2013; de Pablo, Miguel
Angel/J-6442-2014; Hayes, Alexander/P-2024-2014; Gasnault,
Olivier/F-4327-2010; Zorzano, Maria-Paz/C-5784-2015; szopa,
cyril/C-6865-2015; Martin-Torres, Francisco Javier/G-6329-2015; Blanco,
Juan Jose/E-3627-2014; Crisp, Joy/H-8287-2016; Harri,
Ari-Matti/C-7142-2012; Zorzano, Maria-Paz/F-2184-2015; Dworkin,
Jason/C-9417-2012
OI Gomez-Elvira, Javier/0000-0002-9068-9846; Ramos,
Miguel/0000-0003-3648-6818; Gomez, Felipe/0000-0001-9977-7060;
Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Madsen,
Morten/0000-0001-8909-5111; Lemmon, Mark/0000-0002-4504-5136; Glavin,
Daniel/0000-0001-7779-7765; Frydenvang, Jens/0000-0001-9294-1227;
Balic-Zunic, Tonci/0000-0003-1687-1233; de Pablo, Miguel
Angel/0000-0002-4496-2741; Edgett, Kenneth/0000-0001-7197-5751; Muller,
Jan-Peter/0000-0002-5077-3736; Forni, Olivier/0000-0001-6772-9689;
Hayes, Alexander/0000-0001-6397-2630; Gasnault,
Olivier/0000-0002-6979-9012; Zorzano, Maria-Paz/0000-0002-4492-9650;
szopa, cyril/0000-0002-0090-4056; Martin-Torres, Francisco
Javier/0000-0001-6479-2236; Blanco, Juan Jose/0000-0002-8666-0696;
Crisp, Joy/0000-0002-3202-4416; Harri, Ari-Matti/0000-0001-8541-2802;
Zorzano, Maria-Paz/0000-0002-4492-9650; Dworkin,
Jason/0000-0002-3961-8997
FU NASA Mars Science Laboratory Mission; Danish Council for Independent
Research/Natural Sciences (Det Frie Forskningsrad Natur og Univers FNU)
[12-127126, 11-107019]; Deutsche Forschungsgemeinschaft (DFG) [GO
2288/1-1]; NASA
FX Support from the NASA Mars Science Laboratory Mission is gratefully
acknowledged. The chemical and mineralogical data presented here are
derived from the archived data sets in the NASA Planetary Data System
(PDS) http://pds-geosciences.wustl.edu/missions/msl, specifically
MSL-M-CHEMIN-2-EDR-V1.0 and MSL-M-APXS-2-EDR-V1.0. M. B. M. was funded
by the Danish Council for Independent Research/Natural Sciences (Det
Frie Forskningsrad Natur og Univers FNU grants 12-127126 and 11-107019).
W. G. acknowledges partial funding by the Deutsche
Forschungsgemeinschaft (DFG grant GO 2288/1-1). Some of this research
was carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with NASA.
NR 40
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U1 6
U2 111
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 SEP 27
PY 2013
VL 341
IS 6153
AR 1239505
DI 10.1126/science.1239505
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 224NS
UT WOS:000324894600005
PM 24072928
ER
PT J
AU Leshin, LA
Mahaffy, PR
Webster, CR
Cabane, M
Coll, P
Conrad, PG
Archer, PD
Atreya, SK
Brunner, AE
Buch, A
Eigenbrode, JL
Flesch, GJ
Franz, HB
Freissinet, C
Glavin, DP
McAdam, AC
Miller, KE
Ming, DW
Morris, RV
Navarro-Gonzalez, R
Niles, PB
Owen, T
Pepin, RO
Squyres, S
Steele, A
Stern, JC
Summons, RE
Sumner, DY
Sutter, B
Szopa, C
Teinturier, S
Trainer, MG
Wray, JJ
Grotzinger, JP
AF Leshin, L. A.
Mahaffy, P. R.
Webster, C. R.
Cabane, M.
Coll, P.
Conrad, P. G.
Archer, P. D., Jr.
Atreya, S. K.
Brunner, A. E.
Buch, A.
Eigenbrode, J. L.
Flesch, G. J.
Franz, H. B.
Freissinet, C.
Glavin, D. P.
McAdam, A. C.
Miller, K. E.
Ming, D. W.
Morris, R. V.
Navarro-Gonzalez, R.
Niles, P. B.
Owen, T.
Pepin, R. O.
Squyres, S.
Steele, A.
Stern, J. C.
Summons, R. E.
Sumner, D. Y.
Sutter, B.
Szopa, C.
Teinturier, S.
Trainer, M. G.
Wray, J. J.
Grotzinger, J. P.
CA MSL Sci Team
TI Volatile, Isotope, and Organic Analysis of Martian Fines with the Mars
Curiosity Rover
SO SCIENCE
LA English
DT Article
ID PHOENIX LANDING SITE; X-RAY SPECTROMETER; CHEMICAL-COMPOSITION;
PATHFINDER SITE; SNC METEORITES; CHEMISTRY; CARBONATE; ALH84001; SOILS;
ROCKS
AB Samples from the Rocknest aeolian deposit were heated to similar to 835 degrees C under helium flow and evolved gases analyzed by Curiosity's Sample Analysis at Mars instrument suite. H2O, SO2, CO2, and O-2 were the major gases released. Water abundance (1.5 to 3 weight percent) and release temperature suggest that H2O is bound within an amorphous component of the sample. Decomposition of fine-grained Fe or Mg carbonate is the likely source of much of the evolved CO2. Evolved O-2 is coincident with the release of Cl, suggesting that oxygen is produced from thermal decomposition of an oxychloride compound. Elevated delta D values are consistent with recent atmospheric exchange. Carbon isotopes indicate multiple carbon sources in the fines. Several simple organic compounds were detected, but they are not definitively martian in origin.
C1 [Leshin, L. A.] Rensselaer Polytech Inst, Dept Earth & Environm Sci, Troy, NY 12180 USA.
[Leshin, L. A.] Rensselaer Polytech Inst, Sch Sci, Troy, NY 12180 USA.
[Mahaffy, P. R.; Conrad, P. G.; Brunner, A. E.; Eigenbrode, J. L.; Franz, H. B.; Freissinet, C.; Glavin, D. P.; McAdam, A. C.; Stern, J. C.; Trainer, M. G.] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA.
[Webster, C. R.; Flesch, G. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cabane, M.; Szopa, C.; Teinturier, S.] Univ Paris 06, LATMOS, Univ Versailles St Quentin, UMR 8970,CNRS, F-75005 Paris, France.
[Coll, P.] Univ Paris Diderot, Univ Paris Est, LISA, F-94000 Creteil, France.
[Coll, P.] CNRS, F-94000 Creteil, France.
[Archer, P. D., Jr.; Ming, D. W.; Morris, R. V.; Niles, P. B.; 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.
[Brunner, A. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Buch, A.] Ecole Cent Paris, Lab Genie Procedes & Mat, F-92295 Chatenay Malabry, France.
[Franz, H. B.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA.
[Miller, K. E.; Summons, R. E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Navarro-Gonzalez, R.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico.
[Owen, T.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Pepin, R. O.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Squyres, S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Steele, A.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Sumner, D. Y.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA.
[Sutter, B.] Jacobs, Houston, TX 77058 USA.
[Wray, J. J.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Grotzinger, J. P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Leshin, LA (reprint author), Rensselaer Polytech Inst, Dept Earth & Environm Sci, Troy, NY 12180 USA.
EM leshin@rpi.edu
RI Hayes, Alexander/P-2024-2014; Trainer, Melissa/E-1477-2012; Zorzano,
Maria-Paz/C-5784-2015; szopa, cyril/C-6865-2015; Martin-Torres,
Francisco Javier/G-6329-2015; Blanco, Juan Jose/E-3627-2014; Harri,
Ari-Matti/C-7142-2012; Zorzano, Maria-Paz/F-2184-2015; Dworkin,
Jason/C-9417-2012; Wray, James/B-8457-2008; Gonzalez,
Rafael/D-1748-2009; Lemmon, Mark/E-9983-2010; Glavin,
Daniel/D-6194-2012; Stern, Jennifer/E-3135-2012; Frydenvang,
Jens/D-4781-2013; Balic-Zunic, Tonci/A-6362-2013; de Pablo, Miguel
Angel/J-6442-2014; Gomez-Elvira, Javier/K-5829-2014; Ramos,
Miguel/K-2230-2014; Gomez, Felipe/L-7315-2014; Rodriguez-Manfredi,
Jose/L-8001-2014
OI Hayes, Alexander/0000-0001-6397-2630; Zorzano,
Maria-Paz/0000-0002-4492-9650; szopa, cyril/0000-0002-0090-4056;
Martin-Torres, Francisco Javier/0000-0001-6479-2236; Blanco, Juan
Jose/0000-0002-8666-0696; Harri, Ari-Matti/0000-0001-8541-2802; Zorzano,
Maria-Paz/0000-0002-4492-9650; Dworkin, Jason/0000-0002-3961-8997;
Muller, Jan-Peter/0000-0002-5077-3736; Wray, James/0000-0001-5559-2179;
Lemmon, Mark/0000-0002-4504-5136; Glavin, Daniel/0000-0001-7779-7765;
Stern, Jennifer/0000-0002-0162-8807; Frydenvang,
Jens/0000-0001-9294-1227; Balic-Zunic, Tonci/0000-0003-1687-1233; de
Pablo, Miguel Angel/0000-0002-4496-2741; Gomez-Elvira,
Javier/0000-0002-9068-9846; Ramos, Miguel/0000-0003-3648-6818; Gomez,
Felipe/0000-0001-9977-7060; Rodriguez-Manfredi, Jose/0000-0003-0461-9815
NR 48
TC 121
Z9 123
U1 22
U2 157
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD SEP 27
PY 2013
VL 341
IS 6153
AR UNSP 1238937
DI 10.1126/science.1238937
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 224NS
UT WOS:000324894600003
PM 24072926
ER
PT J
AU Meslin, PY
Gasnault, O
Forni, O
Schroder, S
Cousin, A
Berger, G
Clegg, SM
Lasue, J
Maurice, S
Sautter, V
Le Mouelic, S
Wiens, RC
Fabre, C
Goetz, W
Bish, D
Mangold, N
Ehlmann, B
Lanza, N
Harri, AM
Anderson, R
Rampe, E
McConnochie, TH
Pinet, P
Blaney, D
Leveille, R
Archer, D
Barraclough, B
Bender, S
Blake, D
Blank, JG
Bridges, N
Clark, BC
DeFlores, L
Delapp, D
Dromart, G
Dyar, MD
Fisk, M
Gondet, B
Grotzinger, J
Herkenhoff, K
Johnson, J
Lacour, JL
Langevin, Y
Leshin, L
Lewin, E
Madsen, MB
Melikechi, N
Mezzacappa, A
Mischna, MA
Moores, JE
Newsom, H
Ollila, A
Perez, R
Renno, N
Sirven, JB
Tokar, R
de la Torre, M
d'Uston, L
Vaniman, D
Yingst, A
AF Meslin, P-Y.
Gasnault, O.
Forni, O.
Schroeder, S.
Cousin, A.
Berger, G.
Clegg, S. M.
Lasue, J.
Maurice, S.
Sautter, V.
Le Mouelic, S.
Wiens, R. C.
Fabre, C.
Goetz, W.
Bish, D.
Mangold, N.
Ehlmann, B.
Lanza, N.
Harri, A-M.
Anderson, R.
Rampe, E.
McConnochie, T. H.
Pinet, P.
Blaney, D.
Leveille, R.
Archer, D.
Barraclough, B.
Bender, S.
Blake, D.
Blank, J. G.
Bridges, N.
Clark, B. C.
DeFlores, L.
Delapp, D.
Dromart, G.
Dyar, M. D.
Fisk, M.
Gondet, B.
Grotzinger, J.
Herkenhoff, K.
Johnson, J.
Lacour, J-L.
Langevin, Y.
Leshin, L.
Lewin, E.
Madsen, M. B.
Melikechi, N.
Mezzacappa, A.
Mischna, M. A.
Moores, J. E.
Newsom, H.
Ollila, A.
Perez, R.
Renno, N.
Sirven, J-B.
Tokar, R.
de la Torre, M.
d'Uston, L.
Vaniman, D.
Yingst, A.
CA MSL Sci Team
TI Soil Diversity and Hydration as Observed by ChemCam at Gale Crater, Mars
SO SCIENCE
LA English
DT Article
ID EMISSION SPECTROMETER DATA; X-RAY SPECTROMETER; CHEMICAL-COMPOSITION;
INSTRUMENT SUITE; HYDROUS MINERALS; MARTIAN REGOLITH; WATER; SURFACE;
CHEMISTRY; ALLOPHANE
AB The ChemCam instrument, which provides insight into martian soil chemistry at the submillimeter scale, identified two principal soil types along the Curiosity rover traverse: a fine-grained mafic type and a locally derived, coarse-grained felsic type. The mafic soil component is representative of widespread martian soils and is similar in composition to the martian dust. It possesses a ubiquitous hydrogen signature in ChemCam spectra, corresponding to the hydration of the amorphous phases found in the soil by the CheMin instrument. This hydration likely accounts for an important fraction of the global hydration of the surface seen by previous orbital measurements. ChemCam analyses did not reveal any significant exchange of water vapor between the regolith and the atmosphere. These observations provide constraints on the nature of the amorphous phases and their hydration.
C1 [Meslin, P-Y.; Gasnault, O.; Forni, O.; Schroeder, S.; Berger, G.; Lasue, J.; Maurice, S.; Pinet, P.; d'Uston, L.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France.
[Meslin, P-Y.; Gasnault, O.; Forni, O.; Schroeder, S.; Berger, G.; Lasue, J.; Maurice, S.; Pinet, P.; d'Uston, L.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Cousin, A.; Clegg, S. M.; Wiens, R. C.; Lanza, N.; Delapp, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Sautter, V.] Museum Natl Hist Nat, Lab Mineral & Cosmochim Museum, F-75005 Paris, France.
[Le Mouelic, S.; Mangold, N.] Univ Nantes, LPGN, CNRS, UMR6112, F-44322 Nantes, France.
[Fabre, C.] Univ Lorraine, GeoRessources, CNRS, UMR7356, F-54506 Vandoeuvre Les Nancy, France.
[Goetz, W.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Bish, D.] Indiana Univ, Bloomington, IN 47405 USA.
[Ehlmann, B.; Grotzinger, J.; de la Torre, M.] CALTECH, Pasadena, CA 91125 USA.
[Ehlmann, B.; Blaney, D.; DeFlores, L.; Mischna, M. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Harri, A-M.] Finnish Meteorol Inst, Earth Observat Res Div, FIN-00101 Helsinki, Finland.
[Anderson, R.; Herkenhoff, K.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Rampe, E.; Archer, D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[McConnochie, T. H.] Univ Maryland, College Pk, MD 20740 USA.
[Leveille, R.] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada.
[Barraclough, B.; Bender, S.; Tokar, R.; Vaniman, D.; Yingst, A.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Blake, D.; Blank, J. G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Johnson, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Clark, B. C.] Space Sci Inst, Boulder, CO 80301 USA.
[Dromart, G.] ENS, F-69007 Lyon, France.
[Dyar, M. D.] Mt Holyoke Coll, S Hadley, MA 01075 USA.
[Fisk, M.] Oregon State Univ, Corvallis, OR 97331 USA.
[Gondet, B.; Langevin, Y.] Inst Astrophys Spatiale, F-91405 Orsay, France.
[Lacour, J-L.; Sirven, J-B.] Commissariat Energie Atom & Energies Alternat, Ctr Saclay, F-91400 Orsay, France.
[Leshin, L.] Rensselaer Polytech Inst, Troy, NY 12180 USA.
[Lewin, E.] ISTerre, F-38041 Grenoble, France.
[Madsen, M. B.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Melikechi, N.; Mezzacappa, A.] Delaware State Univ, Opt Sci Ctr Appl Res, Dover, DE 19901 USA.
[Moores, J. E.] York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 1P3, Canada.
[Newsom, H.; Ollila, A.] Univ New Mexico, Albuquerque, NM 87131 USA.
[Perez, R.] Ctr Natl Etud Spatiales, F-31400 Toulouse, France.
[Renno, N.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Meslin, PY (reprint author), Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France.
EM pmeslin@irap.omp.eu
RI LEWIN, Eric/F-1451-2017; Hayes, Alexander/P-2024-2014; Gasnault,
Olivier/F-4327-2010; Zorzano, Maria-Paz/C-5784-2015; szopa,
cyril/C-6865-2015; Martin-Torres, Francisco Javier/G-6329-2015; Blanco,
Juan Jose/E-3627-2014; BERGER, Gilles/F-7118-2016; Harri,
Ari-Matti/C-7142-2012; Zorzano, Maria-Paz/F-2184-2015; Dworkin,
Jason/C-9417-2012; Sirven, Jean-Baptiste/H-5782-2013; Gomez-Elvira,
Javier/K-5829-2014; Ramos, Miguel/K-2230-2014; Gomez,
Felipe/L-7315-2014; Rodriguez-Manfredi, Jose/L-8001-2014; Madsen,
Morten/D-2082-2011; Gonzalez, Rafael/D-1748-2009; Lemmon,
Mark/E-9983-2010; Frydenvang, Jens/D-4781-2013; Balic-Zunic,
Tonci/A-6362-2013; de Pablo, Miguel Angel/J-6442-2014
OI Muller, Jan-Peter/0000-0002-5077-3736; Forni,
Olivier/0000-0001-6772-9689; Clegg, Sam/0000-0002-0338-0948; Hayes,
Alexander/0000-0001-6397-2630; Gasnault, Olivier/0000-0002-6979-9012;
Zorzano, Maria-Paz/0000-0002-4492-9650; szopa,
cyril/0000-0002-0090-4056; Martin-Torres, Francisco
Javier/0000-0001-6479-2236; Blanco, Juan Jose/0000-0002-8666-0696;
Harri, Ari-Matti/0000-0001-8541-2802; Zorzano,
Maria-Paz/0000-0002-4492-9650; Dworkin, Jason/0000-0002-3961-8997;
Sirven, Jean-Baptiste/0000-0002-5523-6809; Gomez-Elvira,
Javier/0000-0002-9068-9846; Ramos, Miguel/0000-0003-3648-6818; Gomez,
Felipe/0000-0001-9977-7060; Rodriguez-Manfredi,
Jose/0000-0003-0461-9815; Madsen, Morten/0000-0001-8909-5111; Lemmon,
Mark/0000-0002-4504-5136; Frydenvang, Jens/0000-0001-9294-1227;
Balic-Zunic, Tonci/0000-0003-1687-1233; de Pablo, Miguel
Angel/0000-0002-4496-2741
FU Centre National d'Etudes Spatiales (CNES); NASA's Mars Program Office;
Deutsche Forschungsgemeinschaft [GO 2288/1-1]
FX This research was carried out with funding from the Centre National
d'Etudes Spatiales (CNES). Work in the United States was carried out
under contract from NASA's Mars Program Office. W. G. acknowledges
partial funding from Deutsche Forschungsgemeinschaft grant GO 2288/1-1.
This team gratefully acknowledges JPL for developing and leading this
successful mission. The data reported in this paper are archived at the
Planetary Data System, accessible at
http://pds-geosciences.wustl.edu/missions/msl/index.htm.
NR 64
TC 85
Z9 85
U1 11
U2 145
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD SEP 27
PY 2013
VL 341
IS 6153
AR 1238670
DI 10.1126/science.1238670
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 224NS
UT WOS:000324894600001
PM 24072924
ER
PT J
AU Loop, MS
Kent, ST
Al-Hamdan, MZ
Crosson, WL
Estes, SM
Estes, MG
Quattrochi, DA
Hemmings, SN
Wadley, VG
McClure, LA
AF Loop, Matthew Shane
Kent, Shia T.
Al-Hamdan, Mohammad Z.
Crosson, William L.
Estes, Sue M.
Estes, Maurice G., Jr.
Quattrochi, Dale A.
Hemmings, Sarah N.
Wadley, Virginia G.
McClure, Leslie A.
TI Fine Particulate Matter and Incident Cognitive Impairment in the REasons
for Geographic and Racial Differences in Stroke (REGARDS) Cohort
SO PLOS ONE
LA English
DT Article
ID AIR-POLLUTION EXPOSURE; UNITED-STATES; BRAIN INFLAMMATION; RISK-FACTORS;
US ADULTS; ASSOCIATION; INDIVIDUALS; CHILDREN; AEROSOL; HEALTH
AB Studies of the effect of air pollution on cognitive health are often limited to populations living near cities that have air monitoring stations. Little is known about whether the estimates from such studies can be generalized to the U.S. population, or whether the relationship differs between urban and rural areas. To address these questions, we used a satellite-derived estimate of fine particulate matter (PM2.5) concentration to determine whether PM2.5 was associated with incident cognitive impairment in a geographically diverse, biracial US cohort of men and women (n = 20,150). A 1-year mean baseline PM2.5 concentration was estimated for each participant, and cognitive status at the most recent follow-up was assessed over the telephone using the Six-Item Screener (SIS) in a subsample that was cognitively intact at baseline. Logistic regression was used to determine whether PM2.5 was related to the odds of incident cognitive impairment. A 10 mu g/m(3) increase in PM2.5 concentration was not reliably associated with an increased odds of incident impairment, after adjusting for temperature, season, incident stroke, and length of follow-up [OR (95% CI): 1.26 (0.97, 1.64)]. The odds ratio was attenuated towards 1 after adding demographic covariates, behavioral factors, and known comorbidities of cognitive impairment. A 10 mu g/m(3) increase in PM2.5 concentration was slightly associated with incident impairment in urban areas (1.40 [1.06-1.85]), but this relationship was also attenuated after including additional covariates in the model. Evidence is lacking that the effect of PM2.5 on incident cognitive impairment is robust in a heterogeneous US cohort, even in urban areas.
C1 [Loop, Matthew Shane; McClure, Leslie A.] Univ Alabama Birmingham, Dept Biostat, Birmingham, AL 35294 USA.
[Kent, Shia T.] Univ Alabama Birmingham, Dept Environm Hlth Sci, Birmingham, AL 35294 USA.
[Al-Hamdan, Mohammad Z.; Crosson, William L.; Estes, Sue M.; Estes, Maurice G., Jr.; Hemmings, Sarah N.] NASA Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL USA.
[Quattrochi, Dale A.] NASA Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL USA.
[Wadley, Virginia G.] Univ Alabama Birmingham, Sch Med, Div Gerontol Geriatr & Palliat Care, Birmingham, AL 35294 USA.
RP Loop, MS (reprint author), Univ Alabama Birmingham, Dept Biostat, Birmingham, AL 35294 USA.
EM loop2@uab.edu
RI McClure, Leslie/P-2929-2015;
OI Loop, Matthew/0000-0001-9442-4573
FU National Institute of Neurological Disorders and Stroke [U01NS41588];
National Institutes of Health Heart, Lung and Blood Institute
[T32HL079888]; National Aeronautics and Space Administration
[NNX09AV81G]
FX This work was supported by federal grants from National Institute of
Neurological Disorders and Stroke (U01NS41588,
http://www.ninds.nih.gov/), National Institutes of Health Heart, Lung
and Blood Institute (T32HL079888, http://www.nhlbi.nih.gov/), and
National Aeronautics and Space Administration (NNX09AV81G,
http://www.nasa.gov/). The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 41
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Z9 11
U1 1
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 SEP 25
PY 2013
VL 8
IS 9
AR e75001
DI 10.1371/journal.pone.0075001
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 228VC
UT WOS:000325218700049
PM 24086422
ER
PT J
AU Silk, EA
Myre, D
AF Silk, Eric A.
Myre, David
TI Fractal Loop Heat Pipe performance testing with a compressed carbon foam
wick structure
SO APPLIED THERMAL ENGINEERING
LA English
DT Article
DE Loop Heat Pipe; Foam; Heat pipe; Wick; Thermal conductance
ID OPERATING TEMPERATURE; EVAPORATOR
AB This study investigates heat flux performance for a prototype wick structure fabricated from compressed carbon foam when used with a Loop Heat Pipe (LHP) containing a fractal-based evaporator design. The prototype wick structure geometry was based on a previous soda lime glass wick structure designed and manufactured by Mikros Manufacturing Inc., for use with the Fractal Loop Heat Pipe (FLHP). The compressed carbon foam wick structure was manufactured by ERG Aerospace Inc., and machined to specifications comparable to that of the initial soda lime glass wick structure. Machining of the compressed foam as well as performance testing were performed at the United States Naval Academy's School of Engineering. Heat input to the FLHP was supplied via cartridge heaters mounted in a copper block. The copper heater block was placed in intimate contact with the evaporator. The evaporator had a circular cross-sectional area of 0.88 cm(2). Twice distilled, deionized water was used as the working fluid. Thermal performance data was obtained for three different Condenser/Subcooler temperatures under degassed conditions (P-sat of 10.5 kPa at 23 degrees C). The compressed carbon foam wick structure demonstrated successful start-ups in each of the test cases performed and had a maximum heat flux of 70 W/cm(2). Published by Elsevier Ltd.
C1 [Silk, Eric A.] NASA, Goddard Space Flight Ctr, Cryogen & Fluids Branch, Greenbelt, MD 20771 USA.
[Myre, David] US Naval Acad, Dept Aerosp Engn, Annapolis, MD 20412 USA.
RP Silk, EA (reprint author), NASA, Goddard Space Flight Ctr, Cryogen & Fluids Branch, 8800 Greenbelt Rd,Code 552-0, Greenbelt, MD 20771 USA.
EM eric.a.silk@nasa.gov
FU Cryogenics; Fluids Branch at the NASA Goddard Space Flight Center;
United States Naval Academy's Aerospace Engineering Department
FX Eric Silk was supported by the Cryogenics and Fluids Branch at the NASA
Goddard Space Flight Center. David Myre was supported by the United
States Naval Academy's Aerospace Engineering Department. Special thanks
to Brandon and William Stanley for their efforts and consultation in the
machining of the compressed foam wick structure used in this study.
Special thanks also go to Mark McClendon and NASA Goddard Space Flight
Center's Materials Engineering Branch (Code 541) for their support in
providing SEM photos of the silica glass wick structure. Last but not
least, thanks to ERG Aerospace for providing SEM photos of their
compressed foam structures.
NR 29
TC 7
Z9 7
U1 1
U2 19
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-4311
J9 APPL THERM ENG
JI Appl. Therm. Eng.
PD SEP 25
PY 2013
VL 59
IS 1-2
BP 290
EP 297
DI 10.1016/j.applthermaleng.2013.05.030
PG 8
WC Thermodynamics; Energy & Fuels; Engineering, Mechanical; Mechanics
SC Thermodynamics; Energy & Fuels; Engineering; Mechanics
GA 213RR
UT WOS:000324077800032
ER
PT J
AU Minazzoli, O
AF Minazzoli, Olivier
TI gamma parameter in Brans-Dicke-like (light-)scalar-tensor theory with a
universal scalar-matter coupling
SO PHYSICAL REVIEW D
LA English
DT Article
ID STRING THEORY; GRAVITY; CONSTANT
AB The post-Newtonian parameter gamma resulting from a universal scalar-matter coupling is investigated in Brans-Dicke-like scalar-tensor theories where the scalar potential is assumed to be negligible. Conversely to previous studies, we use a perfect fluid formalism in order to get the explicit scalar-field equation. It is shown that the metric can be put in its standard post-Newtonian form. However, it is pointed out that 1 - gamma could be either positive, null or negative for a finite value of ! 0, depending on the coupling function, while scalar-tensor theories without coupling always predict gamma < 1 for a finite value of omega(0).
C1 [Minazzoli, Olivier] Univ Nice Sophia Antipolis, CNRS, UMR ARTEMIS, Observ Cote Azur, F-06304 Nice 4, France.
[Minazzoli, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Minazzoli, O (reprint author), Univ Nice Sophia Antipolis, CNRS, UMR ARTEMIS, Observ Cote Azur, BP4229, F-06304 Nice 4, France.
OI Minazzoli, Olivier/0000-0002-3151-7593
FU NASA Postdoctoral Program at the Jet Propulsion Laboratory, California
Institute of Technology
FX This research was partly 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 NASA. Government sponsorship is
acknowledged. This research was partly done as an invited researcher of
the Observatoire de la Cote d'Azur. The author wants to thank Aurelien
Hees, Tiberiu Harko, Francisco Lobo, John Moffat, and Viktor Toth for
their interesting comments.
NR 46
TC 5
Z9 5
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 SEP 24
PY 2013
VL 88
IS 6
AR 064050
DI 10.1103/PhysRevD.88.064050
PG 6
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 222VQ
UT WOS:000324760500008
ER
PT J
AU Anderson, MS
AF Anderson, Mark S.
TI Electride mediated surface enhanced Raman scattering
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID INFRARED-ABSORPTION; ANIONS; SPECTROSCOPY; SPECTRA; PHONON; SERS
AB A ceramic electride is demonstrated to provide surface enhanced Raman scattering. The electride, an ionic crystal where the electrons serve as anions, is a conductive ceramic derived from mayenite. The textured electride surface was found to strongly enhance the Raman scattering of an organic analyte at 532 nm and 785 nm excitation wavelengths. This provides a sensitive method for monitoring the chemistry and electronic environment at the electride surface. The results are evidence of a surface electride-polariton resonance mechanism that is analogous to the surface plasmon-polariton resonance that mediates conventional surface enhance Raman scattering. (C) 2013 AIP Publishing LLC.
C1 [Anderson, Mark S.] CALTECH, Jet Prop Lab, Analyt Chem & Mat Dev Grp, Pasadena, CA 91109 USA.
RP Anderson, MS (reprint author), CALTECH, Jet Prop Lab, Analyt Chem & Mat Dev Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Mark.S.Anderson@jpl.nasa.gov
NR 21
TC 3
Z9 3
U1 2
U2 27
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD SEP 23
PY 2013
VL 103
IS 13
AR 131103
DI 10.1063/1.4822111
PG 4
WC Physics, Applied
SC Physics
GA 229RJ
UT WOS:000325284500003
ER
PT J
AU Biswas, R
Blackburn, L
Cao, J
Essick, R
Hodge, KA
Katsavounidis, E
Kim, K
Kim, YM
Le Bigot, EO
Lee, CH
Oh, JJ
Oh, SH
Son, EJ
Tao, Y
Vaulin, R
Wang, X
AF Biswas, Rahul
Blackburn, Lindy
Cao, Junwei
Essick, Reed
Hodge, Kari Alison
Katsavounidis, Erotokritos
Kim, Kyungmin
Kim, Young-Min
Le Bigot, Eric-Olivier
Lee, Chang-Hwan
Oh, John J.
Oh, Sang Hoon
Son, Edwin J.
Tao, Ye
Vaulin, Ruslan
Wang, Xiaoge
TI Application of machine learning algorithms to the study of noise
artifacts in gravitational-wave data
SO PHYSICAL REVIEW D
LA English
DT Article
ID NETWORKS
AB The sensitivity of searches for astrophysical transients in data from the Laser Interferometer Gravitational-wave Observatory (LIGO) is generally limited by the presence of transient, non-Gaussian noise artifacts, which occur at a high enough rate such that accidental coincidence across multiple detectors is non-negligible. These "glitches" can easily be mistaken for transient gravitational-wave signals, and their robust identification and removal will help any search for astrophysical gravitational waves. We apply machine-learning algorithms (MLAs) to the problem, using data from auxiliary channels within the LIGO detectors that monitor degrees of freedom unaffected by astrophysical signals. Noise sources may produce artifacts in these auxiliary channels as well as the gravitational-wave channel. The number of auxiliary-channel parameters describing these disturbances may also be extremely large; high dimensionality is an area where MLAs are particularly well suited. We demonstrate the feasibility and applicability of three different MLAs: artificial neural networks, support vector machines, and random forests. These classifiers identify and remove a substantial fraction of the glitches present in two different data sets: four weeks of LIGO's fourth science run and one week of LIGO's sixth science run. We observe that all three algorithms agree on which events are glitches to within 10% for the sixth-science-run data, and support this by showing that the different optimization criteria used by each classifier generate the same decision surface, based on a likelihood-ratio statistic. Furthermore, we find that all classifiers obtain similar performance to the benchmark algorithm, the ordered veto list, which is optimized to detect pairwise correlations between transients in LIGO auxiliary channels and glitches in the gravitational-wave data. This suggests that most of the useful information currently extracted from the auxiliary channels is already described by this model. Future performance gains are thus likely to involve additional sources of information, rather than improvements in the classification algorithms themselves. We discuss several plausible sources of such new information as well as the ways of propagating it through the classifiers into gravitational-wave searches.
C1 [Biswas, Rahul] Univ Texas Brownsville, Brownsville, TX 78520 USA.
[Blackburn, Lindy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cao, Junwei; Le Bigot, Eric-Olivier] Tsinghua Univ, Tsinghua Natl Lab Informat Sci & Technol, Res Inst Informat Technol, Beijing 100084, Peoples R China.
[Essick, Reed; Katsavounidis, Erotokritos; Vaulin, Ruslan] MIT, LIGO, Cambridge, MA 02139 USA.
[Hodge, Kari Alison] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Kim, Kyungmin] Hanyang Univ, Seoul 133791, South Korea.
[Kim, Kyungmin; Kim, Young-Min; Oh, John J.; Oh, Sang Hoon; Son, Edwin J.] Natl Inst Math Sci, Taejon 305811, South Korea.
[Kim, Young-Min; Lee, Chang-Hwan] Pusan Natl Univ, Pusan 609735, South Korea.
[Tao, Ye; Wang, Xiaoge] Tsinghua Univ, Dept Comp Sci & Technol, Beijing 100084, Peoples R China.
RP Biswas, R (reprint author), Univ Texas Brownsville, Brownsville, TX 78520 USA.
EM vaulin@ligo.mit.edu
RI Lee, Chang-Hwan/B-3096-2015; Biswas, Rahul/H-7474-2016
OI Lee, Chang-Hwan/0000-0003-3221-1171; Biswas, Rahul/0000-0002-0774-8906
FU NASA; Global Science experimental Data hub Center (GSDC) at KISTI;
National Research Foundation Grant; Korean Government
[NRF-2011-220-C00029]; BAERI Nuclear RD program [M20808740002]; Ministry
of Science and Technology of China under the National 973 Basic Research
Program [2011CB302505, 2011CB302805]; National High-Tech Research and
Development Plan of China [2010AA012302]; LIGO laboratory; National
Science Foundation [PHY-0757058]
FX L. B. was supported by an appointment to the NASA Postdoctoral Program
at Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA. K. K., Y. M. K., C. H. L., J.
J. O., S. H. O., and E. J. S. were supported in part by the Global
Science experimental Data hub Center (GSDC) at KISTI. K. K., Y. M. K.,
and C. H. L. were supported in part by National Research Foundation
Grant funded by the Korean Government (NRF-2011-220-C00029). C. H. L.
was supported in part by the BAERI Nuclear R&D program (M20808740002).
J. C., E. O. L., and X. W. were supported in part by the Ministry of
Science and Technology of China under the National 973 Basic Research
Program (Grants No. 2011CB302505 and No. 2011CB302805). T. Y. was
supported in part by the National High-Tech Research and Development
Plan of China (Grant No. 2010AA012302). R. E., K. H., E. K., and R. V.
were supported by LIGO laboratory. LIGO was constructed by the
California Institute of Technology and Massachusetts Institute of
Technology with funding from the National Science Foundation and
operates under cooperative agreement PHY-0757058.
NR 42
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PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD SEP 23
PY 2013
VL 88
IS 6
AR 062003
DI 10.1103/PhysRevD.88.062003
PG 24
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 221WQ
UT WOS:000324691500002
ER
PT J
AU Plante, I
Ponomarev, AL
Cucinotta, FA
AF Plante, Ianik
Ponomarev, Artem L.
Cucinotta, Francis A.
TI Calculation of the energy deposition in nanovolumes by protons and HZE
particles: geometric patterns of initial distributions of DNA repair
foci
SO PHYSICS IN MEDICINE AND BIOLOGY
LA English
DT Article
ID DOUBLE-STRAND BREAKS; HIGH-LET IRRADIATION; IONIZING-RADIATION; TRACK
STRUCTURE; SPATIAL-DISTRIBUTION; MAMMALIAN-CELLS; GAMMA-H2AX FOCI;
DAMAGE; MODEL; INDUCTION
AB The biological effects of high-linear energy transfer (LET) radiation are different from those caused by low-LET radiation due to the difference in the patterns of energy deposition in cells. In this work, we studied the role of the track structure in the spatial distribution of radiation-induced double-strand breaks (DSBs). In the first part, the irradiation of a cubic volume of 12 mu m of side by 300 MeV protons (LET similar to 0.3 keV mu m(-1)) and by 1 GeV/amu iron ion particles (LET similar to 150 keV mu m(-1)) was simulated with the Monte Carlo code RITRACKS (relativistic ion tracks) and the dose was calculated in voxels of different sizes. In the second part, dose calculations were combined with chromosomes simulated by a random walk (RW) model to assess the formation of DSBs. The number of DSBs was calculated as a function of the dose and particle fluence for 1 GeV protons, 293 MeV/u carbon, and 1 GeV/u iron particles. Finally, the DSB yield was obtained as a function of the LET for protons, helium, and carbon. In general, the number and distribution of calculated DSBs were similar to experimental DNA repair foci data. From this study, we concluded that a stochastic model combining nanoscopic dose calculations and chromosomes simulated by RWs is a useful approach to study radiation-induced DSBs.
C1 [Plante, Ianik; Ponomarev, Artem L.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
[Cucinotta, Francis A.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Cucinotta, Francis A.] Univ Nevada, Dept Hlth Phys & Diagnost Sci, Las Vegas, NV 89154 USA.
RP Plante, I (reprint author), Univ Space Res Assoc, Div Space Life Sci, 3600 Bay Area Blvd, Houston, TX 77058 USA.
EM Ianik.Plante-1@nasa.gov
FU National Aeronautics and Space Administration (NASA)
FX Funding for this project was provided through the National Aeronautics
and Space Administration (NASA) Space Radiation Risk Assessment Project.
NR 41
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0031-9155
EI 1361-6560
J9 PHYS MED BIOL
JI Phys. Med. Biol.
PD SEP 21
PY 2013
VL 58
IS 18
BP 6393
EP 6405
DI 10.1088/0031-9155/58/18/6393
PG 13
WC Engineering, Biomedical; Radiology, Nuclear Medicine & Medical Imaging
SC Engineering; Radiology, Nuclear Medicine & Medical Imaging
GA 220HL
UT WOS:000324573400011
PM 23999659
ER
PT J
AU Elkadi, A
Decrossas, E
Yu, SQ
Naseem, HA
El-Ghazaly, SM
AF Elkadi, Asmaa
Decrossas, Emmanuel
Yu, Shui-Q.
Naseem, Hameed A.
El-Ghazaly, Samir M.
TI Aligned semiconducting single-walled carbon nanotubes: Semi-analytical
solution
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID MODEL
AB This paper presents a semi-analytical model to study coupling between adjacent semiconducting single-walled carbon nanotubes (s-SWCNT) and its effect on the energy band gap. A potential function is proposed to describe the charge density distribution of s-SWCNT based on the continuum model. The potential function is then used in solving Schrodinger's equation to obtain the ground state probability wave function for one s-SWCNT and aligned bundle of s-SWCNTs. Then, a parametric study of energy band gap is developed by varying the distance between adjacent s-SWCNTs and applying transverse electric field across the bundle axis. The energy band gap of aligned s-SWCNTs is 10% less than one s-SWCNT. When the distance (d) between the adjacent s-SWCNTs is increased, the change of the energy band gap vanishes. By applying transverse electric field, the energy band gap may reduce by as much as 20% and vanishes with the increase of d. (C) 2013 AIP Publishing LLC.
C1 [Elkadi, Asmaa; Yu, Shui-Q.; Naseem, Hameed A.; El-Ghazaly, Samir M.] Univ Arkansas, Dept Elect Engn, Fayetteville, AR 72701 USA.
[Decrossas, Emmanuel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Elkadi, A (reprint author), Univ Arkansas, Dept Elect Engn, Fayetteville, AR 72701 USA.
EM aelkadi@uark.edu
FU Army Research Laboratory; [W911NF-10-2-0072]
FX This research was sponsored by the Army Research Laboratory and was
accomplished under Cooperative Agreement No. W911NF-10-2-0072. The views
and conclusions contained in this document are those of the authors and
should not be interpreted as representing the official policies, either
expressed or implied, of the Army Research Laboratory or the U. S.
Government. The U. S. Government is authorized to reproduce and
distribute reprints for Government purposes notwithstanding any
copyright notation herein. This work was done as a private venture and
not in the second author's capacity as an employee of the Jet Propulsion
Laboratory, California Institute of Technology.
NR 18
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PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD SEP 21
PY 2013
VL 114
IS 11
AR 114306
DI 10.1063/1.4821272
PG 7
WC Physics, Applied
SC Physics
GA 223RU
UT WOS:000324827200058
ER
PT J
AU Aliu, E
Archambault, S
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bird, R
Bottcher, M
Bouvier, A
Bugaev, V
Byrum, K
Cesarini, A
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Dickherber, R
Duke, C
Dumm, J
Errando, M
Falcone, A
Federici, S
Feng, Q
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Gillanders, GH
Griffin, S
Grube, J
Gyuk, G
Hanna, D
Holder, J
Hughes, G
Humensky, TB
Kaaret, P
Kertzman, M
Khassen, Y
Kieda, D
Krawczynski, H
Krennrich, F
Lang, MJ
Madhavan, AS
Maier, G
Majumdar, P
McArthur, S
McCann, A
Moriarty, P
Mukherjee, R
Nelson, T
de Bhroithe, AO
Ong, RA
Orr, M
Otte, AN
Park, N
Perkins, JS
Pichel, A
Pohl, M
Popkow, A
Prokoph, H
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Saxon, DB
Schroedter, M
Sembroski, GH
Skole, C
Smith, AW
Staszak, D
Telezhinsky, I
Theiling, M
Tyler, J
Varlotta, A
Vassiliev, VV
Wakely, SP
Weekes, TC
Weinstein, A
Welsing, R
Williams, DA
Zitzer, B
AF Aliu, E.
Archambault, S.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Bird, R.
Boettcher, M.
Bouvier, A.
Bugaev, V.
Byrum, K.
Cesarini, A.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Cui, W.
Dickherber, R.
Duke, C.
Dumm, J.
Errando, M.
Falcone, A.
Federici, S.
Feng, Q.
Finley, J. P.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Gillanders, G. H.
Griffin, S.
Grube, J.
Gyuk, G.
Hanna, D.
Holder, J.
Hughes, G.
Humensky, T. B.
Kaaret, P.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
Madhavan, A. S.
Maier, G.
Majumdar, P.
McArthur, S.
McCann, A.
Moriarty, P.
Mukherjee, R.
Nelson, T.
de Bhroithe, A. O'Faolain
Ong, R. A.
Orr, M.
Otte, A. N.
Park, N.
Perkins, J. S.
Pichel, A.
Pohl, M.
Popkow, A.
Prokoph, H.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Saxon, D. B.
Schroedter, M.
Sembroski, G. H.
Skole, C.
Smith, A. W.
Staszak, D.
Telezhinsky, I.
Theiling, M.
Tyler, J.
Varlotta, A.
Vassiliev, V. V.
Wakely, S. P.
Weekes, T. C.
Weinstein, A.
Welsing, R.
Williams, D. A.
Zitzer, B.
TI MULTIWAVELENGTH OBSERVATIONS AND MODELING OF 1ES 1959+650 IN A LOW FLUX
STATE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: general; BL Lacertae objects: individual (1ES
1959+650=VER J1959+651); galaxies: active; gamma rays: galaxies
ID BL-LACERTAE OBJECTS; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; LARGE-AREA
TELESCOPE; GAMMA-RAYS; BLAZAR 1ES-1959+650; RELATIVISTIC JET; SOURCE
CATALOG; LAC OBJECTS; TEV-FLARE; RADIATION
AB We report on the VERITAS observations of the high-frequency peaked BL Lac object 1ES 1959+650 in the period 2007-2011. This source is detected at TeV energies by VERITAS at 16.4 standard deviation (sigma) significance in 7.6 hr of observation in a low flux state. A multiwavelength spectral energy distribution (SED) is constructed from contemporaneous data from VERITAS, Fermi-LAT, RXTE PCA, and Swift UVOT. Swift XRT data is not included in the SED due to a lack of simultaneous observations with VERITAS. In contrast to the orphan gamma-ray flare exhibited by this source in 2002, the X-ray flux of the source is found to vary by an order of magnitude, while other energy regimes exhibit less variable emission. A quasi-equilibrium synchrotron self-Compton model with an additional external radiation field is used to describe three SEDs corresponding to the lowest, highest, and average X-ray states. The variation in the X-ray spectrum is modeled by changing the electron injection spectral index, with minor adjustments of the kinetic luminosity in electrons. This scenario produces small-scale flux variability of the order of less than or similar to 2 in the high energy (E > 1MeV) and very high energy (E > 100 GeV) gamma-ray regimes, which is corroborated by the Fermi-LAT, VERITAS, and Whipple 10 m telescope light curves.
C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Arlen, T.; Aune, T.; Majumdar, P.; Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Beilicke, M.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Bird, R.; Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Boettcher, M.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA.
[Boettcher, M.] North West Univ, Ctr Space Res, ZA-2531 Potchefstroom, South Africa.
[Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
[Dumm, J.; Fortson, L.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Skole, C.; Telezhinsky, I.; Welsing, R.] DESY, D-15738 Zeuthen, Germany.
[Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Finnegan, G.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Gall, D.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Holder, J.; Saxon, D. B.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Saxon, D. B.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Humensky, T. B.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Kertzman, M.] DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India.
[McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
RI Khassen, Yerbol/I-3806-2015;
OI Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772;
Cesarini, Andrea/0000-0002-8611-8610; Lang, Mark/0000-0003-4641-4201;
Bird, Ralph/0000-0002-4596-8563
FU U.S. Department of Energy Office of Science; U.S. National Science
Foundation; Smithsonian Institution; NARC'S in Canada; Science
Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K.; Irish
Research Council "Embark Initiative"
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, by NARC'S in Canada, by Science Foundation
Ireland (SFI 10/RFP/AST2748), 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.; Anna O'Faolain de
Bhroithe acknowledges the support of the Irish Research Council "Embark
Initiative."
NR 59
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
AR 3
DI 10.1088/0004-637X/775/1/3
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800003
ER
PT J
AU Calanog, JA
Wardlow, J
Fu, H
Cooray, A
Assef, RJ
Bock, J
Casey, CM
Conley, A
Farrah, D
Ibar, E
Kartaltepe, J
Magdis, G
Marchetti, L
Oliver, SJ
Perez-Fournon, I
Riechers, D
Rigopoulou, D
Roseboom, IG
Schulz, B
Scott, D
Symeonidis, M
Vaccari, M
Viero, M
Zemcov, M
AF Calanog, J. A.
Wardlow, J.
Fu, Hai
Cooray, A.
Assef, R. J.
Bock, J.
Casey, C. M.
Conley, A.
Farrah, D.
Ibar, E.
Kartaltepe, J.
Magdis, G.
Marchetti, L.
Oliver, S. J.
Perez-Fournon, I.
Riechers, D.
Rigopoulou, D.
Roseboom, I. G.
Schulz, B.
Scott, Douglas
Symeonidis, M.
Vaccari, M.
Viero, M.
Zemcov, M.
TI HerMES: THE FAR-INFRARED EMISSION FROM DUST-OBSCURED GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: luminosity function, mass function; galaxies: star formation;
infrared: galaxies
ID SIMILAR-TO 2; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMING GALAXIES;
ACTIVE GALACTIC NUCLEUS; DEEP-FIELD-SOUTH; SPITZER-SPACE-TELESCOPE;
HERSCHEL-SPIRE INSTRUMENT; HIGH-REDSHIFT; SUBMILLIMETER GALAXIES;
MASSIVE GALAXIES
AB Dust-obscured galaxies (DOGs) are an ultraviolet-faint, infrared-bright galaxy population that reside at z similar to 2 and are believed to be in a phase of dusty star-forming and active galactic nucleus (AGN) activity. We present far-infrared (far-IR) observations of a complete sample of DOGs in the 2 deg(2) of the Cosmic Evolution Survey. The 3077 DOGs have < z > = 1.9 +/- 0.3 and are selected from 24 mu m and r(+) observations using a color cut of r(+) -[24] >= 7.5 (AB mag) and S-24 >= 100 mu Jy. Based on the near-IR spectral energy distributions, 47% are bump DOGs (star formation dominated) and 10% are power-law DOGs (AGN-dominated). We use SPIRE far-IR photometry from the Herschel Multi-tiered Extragalactic Survey to calculate the IR luminosity and characteristic dust temperature for the 1572 (51%) DOGs that are detected at 250 mu m (>= 3 sigma). For the remaining 1505 (49%) that are undetected, we perform a median stacking analysis to probe fainter luminosities. Herschel-detected and undetected DOGs have average luminosities of (2.8 +/- 0.4) x 10(12) L-circle dot and (0.77 +/- 0.08) x 10(12) L-circle dot, and dust temperatures of (33 +/- 7) K and (37 +/- 5) K, respectively. The IR luminosity function for DOGs with S-24 >= 100 mu Jy is calculated, using far-IR observations and stacking. DOGs contribute 10%-30% to the total star formation rate (SFR) density of the universe at z = 1.5-2.5, dominated by 250 mu m detected and bump DOGs. For comparison, DOGs contribute 30% to the SFR density for all z = 1.5-2.5 galaxies with S-24 >= 100 mu Jy. DOGs have a large scatter about the star formation main sequence and their specific SFRs show that the observed phase of star formation could be responsible for their total observed stellar mass at z similar to 2.
C1 [Calanog, J. A.; Wardlow, J.; Fu, Hai; Cooray, A.; Rigopoulou, D.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Fu, Hai] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Cooray, A.; Bock, J.; Riechers, D.; Schulz, B.; Viero, M.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA.
[Assef, R. J.; Bock, J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Casey, C. M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA.
[Farrah, D.; Oliver, S. J.; Roseboom, I. G.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Ibar, E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Kartaltepe, J.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Magdis, G.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Marchetti, L.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Marchetti, L.; Vaccari, M.] Univ Padua, Dipartimento Fis & Astron, Vicolo Osservatorio, I-35122 Padua, Italy.
[Perez-Fournon, I.] Inst Astrofis Canarias IAC, E-38200 Tenerife, Spain.
[Perez-Fournon, I.] Univ La Laguna ULL, Dept Astrofis, E-38205 Tenerife, Spain.
[Rigopoulou, D.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England.
[Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Schulz, B.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa.
RP Calanog, JA (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
RI Magdis, Georgios/C-7295-2014; Wardlow, Julie/C-9903-2015; Vaccari,
Mattia/R-3431-2016;
OI Magdis, Georgios/0000-0002-4872-2294; Wardlow,
Julie/0000-0003-2376-8971; Vaccari, Mattia/0000-0002-6748-0577; Scott,
Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621;
Casey, Caitlin/0000-0002-0930-6466
FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France);
ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA
(USA); NASA; GAANN fellowship; NSF CAREER [AST-0645427]; Science and
Technology Facilities Council [ST/I000976/1]; W. M. Keck Foundation
FX SPIRE has been developed by a consortium of institutes led by Cardiff
University (UK) and including: University of Lethbridge (Canada); NAOC
(China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC
(Spain); Stockholm Observatory (Sweden); Imperial College London, RAL,
UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, University
of 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).; We our thankful to the COSMOS collaboration for granting us
access to their catalogs and we gratefully acknowledge the contributions
of the entire COSMOS team that have made this work possible. More
information on the COSMOS survey is available at
http://hermes.sussex.ac.uk/. 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. We acknowledge support from a GAANN fellowship (to
J.A.C.), NSF CAREER AST-0645427 (A.C. and H.F.), and NASA funds to the
US HerMES team through JPL. S.O. acknowledges support from the Science
and Technology Facilities Council [grant number ST/I000976/1].; Some of
the data (spectroscopic redshifts) 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 the National Aeronautics and Space Administration. The
Observatory was made possible by the generous financial support of the
W. M. Keck Foundation. 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.
NR 93
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
AR 61
DI 10.1088/0004-637X/775/1/61
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800061
ER
PT J
AU Denney, KD
Pogge, RW
Assef, RJ
Kochanek, CS
Peterson, BM
Vestergaard, M
AF Denney, K. D.
Pogge, R. W.
Assef, R. J.
Kochanek, C. S.
Peterson, B. M.
Vestergaard, M.
TI C IV LINE-WIDTH ANOMALIES: THE PERILS OF LOW SIGNAL-TO-NOISE SPECTRA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: nuclei; quasars: emission lines
ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; BLACK-HOLE MASS; AGN
MONITORING PROJECT; VELOCITY-DELAY MAPS; RADIUS-LUMINOSITY RELATIONSHIP;
SEYFERT 1 GALAXIES; EMISSION-LINE; 3C 390.3; ULTRAVIOLET OBSERVATIONS
AB Comparison of six high-redshift quasar spectra obtained with the Large Binocular Telescope with previous observations from the Sloan Digital Sky Survey shows that failure to correctly identify absorption and other problems with accurate characterization of the C IV lambda 1549 emission line profile in low signal-to-noise (S/N) data can severely limit the reliability of single-epoch mass estimates based on the C IV emission line. We combine the analysis of these new high-quality data with a reanalysis of three other samples based on high-S/N spectra of the C IV emission line region. We find that a large scatter between the H beta- and C IV-based masses remains even for this high-S/N sample when using the FWHM to characterize the broad-line region velocity dispersion and the standard virial assumption to calculate the mass. However, we demonstrate that using high-quality data and the line dispersion to characterize the C IV line width leads to a high level of consistency between C IV- and H beta-based masses, with <0.3 dex of observed scatter and an estimated similar to 0.2 dex intrinsic scatter, in the mass residuals.
C1 [Denney, K. D.; Vestergaard, M.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Pogge, R. W.; Kochanek, C. S.; Peterson, B. M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Assef, R. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kochanek, C. S.; Peterson, B. M.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Vestergaard, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Vestergaard, M.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
RP Denney, KD (reprint author), Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
EM kelly@dark-cosmology.dk
RI Vestergaard, Marianne/M-5247-2014
OI Vestergaard, Marianne/0000-0001-9191-9837
FU People Programme (Marie Curie Actions) of the European Union's Seventh
Framework Programme under REA grant [300553]; Space Telescope Science
Institute; NASA [NAS5-26555]; NSF [AST-1009756, AST-1008882,
AST-9987045]; Danish National Research Foundation; NSF Telescope System
Instrumentation Program (TSIP); Ohio Board of Regents; Ohio State
University Office of Research; [HST-AR-12149]
FX We would like to thank Matthias Dietrich for providing C IV spectra for
the objects from the D09 sample presented here. K.D.D. acknowledges
support from the People Programme (Marie Curie Actions) of the European
Union's Seventh Framework Programme FP7/2007-2013/ under REA grant
agreement No. 300553. K.D.D., B.M.P., and M.V. acknowledge support from
grant HST-AR-12149 awarded by the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in
Astronomy, Inc., for NASA, under contract NAS5-26555. R.J.A. is
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. C.S.K. is supported by NSF grant
AST-1009756. B.M.P. and R.W.P. are grateful for NSF support through
grant AST-1008882 to The Ohio State University. The Dark Cosmology
Centre is funded by the Danish National Research Foundation. 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. This work was based in part on
observations made with the Large Binocular Telescope. The LBT is an
international collaboration among institutions in the United States,
Italy, and Germany. The LBT Corporation partners are: the University of
Arizona on behalf of the Arizona university system; the Istituto
Nazionale di Astrofisica, Italy; the LBT Beteiligungsgesellschaft,
Germany, representing the Max Planck Society, the Astrophysical
Institute Potsdam, and Heidelberg University; the Ohio State University;
and the Research Corporation, on behalf of the University of Notre Dame,
the University of Minnesota, and the University of Virginia.
NR 98
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U1 0
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 SEP 20
PY 2013
VL 775
IS 1
AR 60
DI 10.1088/0004-637X/775/1/60
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800060
ER
PT J
AU Fortney, JJ
Mordasini, C
Nettelmann, N
Kempton, EMR
Greene, TP
Zahnle, K
AF Fortney, Jonathan J.
Mordasini, Christoph
Nettelmann, Nadine
Kempton, Eliza M. -R.
Greene, Thomas P.
Zahnle, Kevin
TI A FRAMEWORK FOR CHARACTERIZING THE ATMOSPHERES OF LOW-MASS LOW-DENSITY
TRANSITING PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites:
composition; planets and satellites: formation
ID EARTH GJ 1214B; HUBBLE-SPACE-TELESCOPE; INFRARED TRANSMISSION
SPECTROSCOPY; METAL-RICH ATMOSPHERE; EQUATION-OF-STATE; SUPER-EARTH;
GIANT PLANETS; HOT-NEPTUNE; EXTRASOLAR PLANET; INTERIOR STRUCTURE
AB We perform modeling investigations to aid in understanding the atmospheres and composition of small planets of similar to 2-4 Earth radii, which are now known to be common in our Galaxy. GJ 1214b is a well-studied example whose atmospheric transmission spectrum has been observed by many investigators. Here we take a step back from GJ 1214b to investigate the role that planetary mass, composition, and temperature play in impacting the transmission spectra of these low-mass low-density (LMLD) planets. Under the assumption that these planets accrete modest hydrogen-dominated atmospheres and planetesimals, we use population synthesis models to show that predicted metal enrichments of the H/He envelope are high, with metal mass fraction Z(env) values commonly 0.6-0.9, or similar to 100-400+ times solar. The high mean molecular weight of such atmospheres (mu approximate to 5-12) would naturally help to flatten the transmission spectrum of most LMLD planets. The high metal abundance would also provide significant condensible material for cloud formation. It is known that the H/He abundance in Uranus and Neptune decreases with depth, and we show that atmospheric evaporation of LMLD planets could expose atmospheric layers with gradually higher Z(env). However, values of Z(env) close to solar composition can also arise, so diversity should be expected. Photochemically produced hazes, potentially due to methane photolysis, are another possibility for obscuring transmission spectra. Such hazes may not form above T-eq of similar to 800-1100 K, which is testable if such warm, otherwise low mean molecular weight atmospheres are stable against atmospheric evaporation. We find that available transmission data are consistent with relatively high mean molecular weight atmospheres for GJ 1214b and "warm Neptune" GJ 436b. We examine future prospects for characterizing GJ 1214b with Hubble and the James Webb Space Telescope.
C1 [Fortney, Jonathan J.; Nettelmann, Nadine] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Mordasini, Christoph] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Kempton, Eliza M. -R.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
[Greene, Thomas P.; Zahnle, Kevin] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
RP Fortney, JJ (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
EM jfortney@ucolick.org
OI Fortney, Jonathan/0000-0002-9843-4354
FU NASA [NNX09AC22G, NNX12AI43A, HST-GO-12251.05]
FX J.J.F. acknowledges support from NASA awards NNX09AC22G, NNX12AI43A, and
HST-GO-12251.05. We had many helpful conversations with Mark Marley,
Caroline Morley, and Eric Lopez. We thank the anonymous referee, Brad
Hansen, and Johanna Teske for valuable comments on an earlier draft.
NR 142
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U1 2
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 SEP 20
PY 2013
VL 775
IS 1
AR 80
DI 10.1088/0004-637X/775/1/80
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800080
ER
PT J
AU Garcia, J
Elhoussieny, EE
Bautista, MA
Kallman, TR
AF Garcia, J.
Elhoussieny, E. E.
Bautista, M. A.
Kallman, T. R.
TI TIME-DEPENDENT PHOTOIONIZATION OF GASEOUS NEBULAE: THE PURE HYDROGEN
CASE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: nuclei; galaxies: Seyfert; HII regions; methods: numerical;
planetary nebulae: general; plasmas; quasars: general
ID INTERGALACTIC MEDIUM; INTERSTELLAR-MEDIUM; MODEL ATMOSPHERES; GALAXY
FORMATION; IONIZATION; EVOLUTION; RADIATION; EMISSION; FEEDBACK; SPECTRA
AB We study the problem of time-dependent photoionization of low density gaseous nebulae subjected to sudden changes in the intensity of ionizing radiation. To this end, we write a computer code that solves the full time-dependent energy balance, ionization balance, and radiation transfer equations in a self-consistent fashion for a simplified pure hydrogen case. It is shown that changes in the ionizing radiation yield ionization/thermal fronts that propagate through the cloud, but the propagation times and response times to such fronts vary widely and nonlinearly from the illuminated face of the cloud to the ionization front (IF). IF/thermal fronts are often supersonic, and in slabs initially in pressure equilibrium such fronts yield large pressure imbalances that are likely to produce important dynamical effects in the cloud. Further, we studied the case of periodic variations in the ionizing flux. It is found that the physical conditions of the plasma have complex behaviors that differ from any steady-state solution. Moreover, even the time average of ionization and temperature is different from any steady-state case. This time average is characterized by overionization and a broader IF with respect to the steady-state solution for a mean value of the radiation flux. Around the time average of physical conditions there is a large dispersion in instantaneous conditions, particularly across the IF, which increases with the period of radiation flux variations. Moreover, the variations in physical conditions are asynchronous along the slab due to the combination of nonlinear propagation times for thermal fronts/IFs and equilibration times.
C1 [Garcia, J.; Elhoussieny, E. E.; Bautista, M. A.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA.
[Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Garcia, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM javier@head.cfa.harvard.edu; ehab.elhoussieny@wmich.edu;
manuel.bautista@wmich.edu; timothy.r.kallman@nasa.gov
NR 40
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U1 0
U2 2
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
AR 8
DI 10.1088/0004-637X/775/1/8
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800008
ER
PT J
AU Gies, DR
Guo, Z
Howell, SB
Still, MD
Boyajian, TS
Hoekstra, AJ
Jek, KJ
LaCourse, D
Winarski, T
AF Gies, Douglas R.
Guo, Zhao
Howell, Steve B.
Still, Martin D.
Boyajian, Tabetha S.
Hoekstra, Abe J.
Jek, Kian J.
LaCourse, Daryll
Winarski, Troy
TI KIC 9406652: AN UNUSUAL CATACLYSMIC VARIABLE IN THE KEPLER FIELD OF VIEW
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: spectroscopic; circumstellar matter; novae, cataclysmic
variables; stars: individual (KIC 9406652)
ID X-RAY BINARIES; INTERSTELLAR EXTINCTION; WAVELET ANALYSIS; DONOR STARS;
V344 LYRAE; EVOLUTION; SPECTROSCOPY; SPECTRA; MAJORIS
AB KIC 9406652 is a remarkable variable star in the Kepler field of view that shows both very rapid oscillations and long term outbursts in its light curve. We present an analysis of the light curve over quarters 1-15 and new spectroscopy that indicates that the object is a cataclysmic variable with an orbital period of 6.108 hr. However, an even stronger signal appears in the light curve periodogram for a shorter period of 5.753 hr, and we argue that this corresponds to the modulation of flux from the hot spot region in a tilted, precessing disk surrounding the white dwarf star. We present a preliminary orbital solution from radial velocity measurements of features from the accretion disk and the photosphere of the companion. We use a Doppler tomography algorithm to reconstruct the disk and companion spectra, and we also consider how these components contribute to the object's spectral energy distribution from ultraviolet to infrared wavelengths. This target offers us a remarkable opportunity to investigate disk processes during the high mass transfer stage of evolution in cataclysmic variables.
C1 [Gies, Douglas R.; Guo, Zhao] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA.
[Gies, Douglas R.; Guo, Zhao] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA.
[Howell, Steve B.; Still, Martin D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Still, Martin D.] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
[Boyajian, Tabetha S.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Hoekstra, Abe J.; Jek, Kian J.; LaCourse, Daryll; Winarski, Troy] Yale Univ, Planet Hunters Program, New Haven, CT 06520 USA.
RP Gies, DR (reprint author), Georgia State Univ, Ctr High Angular Resolut Astron, POB 5060, Atlanta, GA 30302 USA.
EM gies@chara.gsu.edu; guo@chara.gsu.edu; steve.b.howell@nasa.gov;
martin.still@nasa.gov; tabetha.boyajian@yale.edu;
abejhoekstra@hotmail.com; kianjin@gmail.com; daryll.lacourse@gmail.com;
troywinarski@gmail.com
OI Boyajian, Tabetha/0000-0001-9879-9313
FU NASA Science Mission Directorate; NASA [NAS5-26555, NNX12AC81G]; NASA
Office of Space Science [NNX09AF08G]; National Science Foundation
[AST-1009080]
FX We thank all the participants of the Planet Hunters program for their
efforts in finding objects like this one. We also express our thanks to
Kimberly Sokal and Phil Massey for helping obtain the first spectra and
to Sergio Dieterich and Richard Wade for their advice with the analysis.
This paper includes data collected by the Kepler mission. Funding for
the Kepler mission is provided by the NASA Science Mission Directorate.
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. Our work was supported in part by NASA grant
NNX12AC81G (D.R.G.) and by the National Science Foundation under grant
AST-1009080 (D.R.G.). Institutional support has been provided from the
GSU College of Arts and Sciences and the Research Program Enhancement
fund of the Board of Regents of the University System of Georgia,
administered through the GSU Office of the Vice President for Research
and Economic Development.
NR 38
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U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
AR 64
DI 10.1088/0004-637X/775/1/64
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800064
ER
PT J
AU Kalas, P
Graham, JR
Fitzgerald, MP
Clampin, M
AF Kalas, Paul
Graham, James R.
Fitzgerald, Michael P.
Clampin, Mark
TI STIS CORONAGRAPHIC IMAGING OF FOMALHAUT: MAIN BELT STRUCTURE AND THE
ORBIT OF FOMALHAUT b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrometry; circumstellar matter; planet-disk interactions; stars:
individual (Fomalhaut)
ID ECCENTRIC EXTRASOLAR PLANETS; HAUMEAS COLLISIONAL FAMILY; SCATTERED
KUIPER-BELT; GIANT IMPACT ORIGIN; SHOEMAKER-LEVY 9; DEBRIS DISK;
SOLAR-SYSTEM; SPACE-TELESCOPE; BETA-PICTORIS; IRREGULAR SATELLITES
AB We present new optical coronagraphic data of Fomalhaut obtained with HST/STIS in 2010 and 2012. Fomalhaut b is recovered at both epochs to high significance. The observations include the discoveries of tenuous nebulosity beyond the main dust belt detected to at least 209 AU projected radius, and a similar to 50AU wide azimuthal gap in the belt northward of Fomalhaut b. The two epochs of Space Telescope Imaging Spectrograph (STIS) photometry exclude optical variability greater than 35%. A Markov chain Monte Carlo analysis demonstrates that the orbit of Fomalhaut b is highly eccentric, with e = 0.8 +/- 0.1, a = 177 +/- 68AU, and q = 32 +/- 24AU. Fomalhaut b is apsidally aligned with the belt and 90% of allowed orbits have mutual inclination <= 36 degrees. Fomalhaut b's orbit is belt crossing in the sky plane projection, but only 12% of possible orbits have ascending or descending nodes within a 25 AU wide belt annulus. The high eccentricity invokes a dynamical history where Fomalhaut b may have experienced a significant dynamical interaction with a hypothetical planet Fomalhaut c, and the current orbital configuration may be relatively short-lived. The Tisserand parameter with respect to a hypothetical Fomalhaut planet at 30 AU or 120 AU lies in the range 2-3, similar to highly eccentric dwarf planets in our solar system. We argue that Fomalhaut b's minimum mass is that of a dwarf planet in order for a circumplanetary satellite system to remain bound to a sufficient radius from the planet to be consistent with the dust scattered light hypothesis. In the coplanar case, Fomalhaut b will collide with the main belt around 2032, and the subsequent emergent phenomena may help determine its physical nature.
C1 [Kalas, Paul; Graham, James R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Kalas, Paul] SETI Inst, Mountain View, CA 94043 USA.
[Graham, James R.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON, Canada.
[Fitzgerald, Michael P.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA.
[Clampin, Mark] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kalas, P (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
RI Fitzgerald, Michael/C-2642-2009
OI Fitzgerald, Michael/0000-0002-0176-8973
FU NASA [NAS5-26555, GO-11818, GO-12576]; STScI under NASA [NAS5-26555];
NSF [AST-0909188]; University of California [LFRP-118057]
FX Based on observations with the NASA/ESA Hubble Space Telescope, obtained
at STScI, which is operated by AURA under NASA contract NAS5-26555. This
work received support from the following: GO-11818 and GO-12576 provided
by NASA through a grant from STScI under NASA contract NAS5-26555; NSF
AST-0909188; and the University of California LFRP-118057. We are
grateful to G. Soutchkova, J. Debes, G. Schneider, J. Duval, A. Aloisi
and C. Proffit for assistance in the observations. We thank H. Beust for
sharing his insights on the Markov chain orbital element analysis, and
A. Jackson, G. Kennedy, H. Levison and M. Wyatt for reviewing the draft
manuscript. We also thank E. Chiang, T. Currie, R. Dawson, G. Duchene,
E. Ford, B. Hansen, M. Hughes, C. Lisse, R. Malhotra, D. Nesvorny, S.
Stewart, D. Tamayo for helpful discussions
NR 163
TC 68
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U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
AR 56
DI 10.1088/0004-637X/775/1/56
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800056
ER
PT J
AU Kay, C
Opher, M
Evans, RM
AF Kay, C.
Opher, M.
Evans, R. M.
TI FORECASTING A CORONAL MASS EJECTION'S ALTERED TRAJECTORY: ForeCAT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: coronal mass ejections (CMEs)
ID IN-SITU OBSERVATIONS; SOLAR-WIND; MAGNETIC-FIELD; STEREO; ACCELERATION;
PROPAGATION; DEFLECTION; MODEL; CYCLE; STRENGTH
AB To predict whether a coronal mass ejection (CME) will impact Earth, the effects of the background on the CME's trajectory must be taken into account. We develop a model, ForeCAT (Forecasting a CME's Altered Trajectory), of CME deflection due to magnetic forces. ForeCAT includes CME expansion, a three-part propagation model, and the effects of drag on the CME's deflection. Given the background solar wind conditions, the launch site of the CME, and the properties of the CME (mass, final propagation speed, initial radius, and initialmagnetic strength), ForeCAT predicts the deflection of the CME. Two different magnetic backgrounds are considered: a scaled background based on type II radio burst profiles and a potential field source surface (PFSS) background. For a scaled background where the CME is launched from an active region located between a coronal hole and streamer region, the strong magnetic gradients cause a deflection of 8.degrees 1 in latitude and 26.degrees 4 in longitude for a 10(15) g CME propagating out to 1 AU. Using the PFSS background, which captures the variation of the streamer belt (SB) position with height, leads to a deflection of 1.degrees 6 in latitude and 4.degrees 1 in longitude for the control case. Varying the CME's input parameters within observed ranges leads to the majority of CMEs reaching the SB within the first few solar radii. For these specific backgrounds, the SB acts like a potential well that forces the CME into an equilibrium angular position.
C1 [Kay, C.; Opher, M.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Evans, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kay, C (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA.
EM ckay@bu.edu
FU NSF CAREER [ATM-0747654]; NASA Postdoctoral Program at GSFC; NASA
FX The authors would like to thank the anonymous referee for his/her
comments. C.K. is supported by NSF CAREER ATM-0747654. R.M.E. is
supported through an appointment to the NASA Postdoctoral Program at
GSFC, administered by Oak Ridge Associated Universities through a
contract with NASA.
NR 71
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U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
AR 5
DI 10.1088/0004-637X/775/1/5
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800005
ER
PT J
AU Kramar, M
Inhester, B
Lin, H
Davila, J
AF Kramar, M.
Inhester, B.
Lin, H.
Davila, J.
TI VECTOR TOMOGRAPHY FOR THE CORONAL MAGNETIC FIELD. II. HANLE EFFECT
MEASUREMENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; polarization; Sun: corona; Sun: infrared
ID EMISSION-LINE POLARIZATION; ILL-POSED PROBLEMS; SOLAR CORONA; FE-XIII;
L-CURVE
AB In this paper, we investigate the feasibility of saturated coronal Hanle effect vector tomography or the application of vector tomographic inversion techniques to reconstruct the three-dimensional magnetic field configuration of the solar corona using linear polarization measurements of coronal emission lines. We applied Hanle effect vector tomographic inversion to artificial data produced from analytical coronal magnetic field models with equatorial and meridional currents and global coronal magnetic field models constructed by extrapolation of real photospheric magnetic field measurements. We tested tomographic inversion with only Stokes Q, U, electron density, and temperature inputs to simulate observations over large limb distances where the Stokes I parameters are difficult to obtain with ground-based coronagraphs. We synthesized the coronal linear polarization maps by inputting realistic noise appropriate for ground-based observations over a period of two weeks into the inversion algorithm. We found that our Hanle effect vector tomographic inversion can partially recover the coronal field with a poloidal field configuration, but that it is insensitive to a corona with a toroidal field. This result demonstrates that Hanle effect vector tomography is an effective tool for studying the solar corona and that it is complementary to Zeeman effect vector tomography for the reconstruction of the coronal magnetic field.
C1 [Kramar, M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Kramar, M.; Davila, J.] NASA GSFC, Greenbelt, MD 20771 USA.
[Inhester, B.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Lin, H.] Univ Hawaii Manoa, Inst Astron, Maui, HI 96768 USA.
RP Kramar, M (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave NE, Washington, DC 20064 USA.
EM maxim.i.kramar@nasa.gov; inhester@mps.mpg.de; lin@ifa.hawaii.edu;
Joseph.M.Davila@nasa.gov
FU NSF National Space Weather Program [AGS0819971]
FX The authors thank the anonymous referee for the insightful review of our
manuscript. This research was supported by NSF National Space Weather
Program grant number AGS0819971.
NR 36
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
AR 25
DI 10.1088/0004-637X/775/1/25
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800025
ER
PT J
AU Lau, RM
Herter, TL
Morris, MR
Becklin, EE
Adams, JD
AF Lau, R. M.
Herter, T. L.
Morris, M. R.
Becklin, E. E.
Adams, J. D.
TI SOFIA/FORCAST IMAGING OF THE CIRCUMNUCLEAR RING AT THE GALACTIC CENTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust; extinction; Galaxy: center; infrared: ISM; photon-dominated region
(PDR)
ID PASCHEN-ALPHA SURVEY; MASSIVE BLACK-HOLE; NE-II OBSERVATIONS;
NEUTRAL-GAS DISK; IONIZED-GAS; SAGITTARIUS-A; STELLAR ORBITS; CENTRAL
PARSEC; GALAXY; RESOLUTION
AB We present 19.7, 31.5, and 37.1 mu m images of the inner 6 pc of the Galactic center of the Milky Way with a spatial resolution of 3.''2-4.''6 taken by the Faint Object Infrared Camera on the Stratospheric Observatory for Infrared Astronomy. The images reveal in detail the "clumpy" structure of the circumnuclear ring (CNR)-the inner edge of the molecular torus orbiting the supermassive black hole at the Galactic center-and the prominent streamers of hot, ionized gas and dust within the CNR that compose the H II region Sgr A West. The CNR exhibits features of a classic H II region: the dust emission at 19.7 mu m closely traces the ionized gas emission observed in the radio while the 31.5 and 37.1 mu m emission traces the photo-dissociation region beyond the ionized gas. The 19.7/37.1 color temperature map reveals a radial temperature gradient across the CNR with temperatures ranging from 65 to 85 K, consistent with the prevailing paradigm in which the dust is centrally heated by the inner cluster of hot, young stars. We model the 37.1 mu m intensity of the CNR as an inclined (theta(i) = 67 degrees) ring with a thickness and radius of 0.34 pc and 1.4 pc, respectively, and find that it is consistent with the observed 37.1 mu m map of the CNR. The 37.1 mu m optical depth map also reveals the clumpy dust distribution of the CNR and implies a total gas mass of similar to 610M(circle dot) . Dense (5-9 x 10(4) cm(-3)) clumps with an FWHM of similar to 0.15 pc exist along the inner edge of the CNR and shadow the material deeper into the ring. We find that the clumps are unlikely to be long-lived structures since they are not dense enough to be stable against tidal shear from the supermassive black hole and will be sheared out on a timescale of an orbital period (similar to 10(5) yr).
C1 [Lau, R. M.; Herter, T. L.; Adams, J. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Morris, M. R.; Becklin, E. E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Becklin, E. E.] Univ Space Res Assoc, Ames Res Ctr, NASA, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
RP Lau, RM (reprint author), Cornell Univ, Dept Astron, 202 Space Sci Bldg, Ithaca, NY 14853 USA.
FU NASA [8500-98-014, NAS2-97001]; Deutsches SOFIA Institut (DSI) under DLR
[50OK 0901]
FX We would like to thank the rest of the FORCAST team, George Gull, Justin
Schoenwald, Chuck Henderson, and Jason Wang, the USRA Science and
Mission Ops teams, and the entire SOFIA staff. We would also thank Hans
Zinnecker and the referee for their valuable comments. This work is
based on observations made with the NASA/DLR Stratospheric Observatory
for Infrared Astronomy (SOFIA). SOFIA Science Mission Operations are
conducted jointly by the Universities Space Research Association, Inc.
(USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut
(DSI) under DLR contract 50OK 0901. Financial support for FORCAST was
provided by NASA through award 8500-98-014 issued by USRA.
NR 46
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
AR 37
DI 10.1088/0004-637X/775/1/37
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800037
ER
PT J
AU Lyra, W
Lin, MK
AF Lyra, Wladimir
Lin, Min-Kai
TI STEADY STATE DUST DISTRIBUTIONS IN DISK VORTICES: OBSERVATIONAL
PREDICTIONS AND APPLICATIONS TO TRANSITIONAL DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: analytical; planet-disk interactions; planets and satellites:
formation; protoplanetary disks
ID ROSSBY-WAVE INSTABILITY; GLOBAL BAROCLINIC INSTABILITY; DIFFERENTIALLY
ROTATING-DISKS; PRIMORDIAL SOLAR NEBULA; MAIN-SEQUENCE STARS; T-TAURI
STARS; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; PLANET FORMATION;
ACCRETION DISKS
AB The Atacama Large Millimeter Array has returned images of transitional disks in which large asymmetries are seen in the distribution of millimeter sized dust in the outer disk. The explanation in vogue borrows from the vortex literature and suggests that these asymmetries are the result of dust trapping in giant vortices, excited via Rossby wave instabilities at planetary gap edges. Due to the drag force, dust trapped in vortices will accumulate in the center and diffusion is needed to maintain a steady state over the lifetime of the disk. While previous work derived semi-analytical models of the process, in this paper we provide analytical steady-steady solutions. Exact solutions exist for certain vortex models. The solution is determined by the vortex rotation profile, the gas scale height, the vortex aspect ratio, and the ratio of dust diffusion to gas-dust friction. In principle, all of these quantities can be derived from observations, which would validate the model and also provide constrains on the strength of the turbulence inside the vortex core. Based on our solution, we derive quantities such as the gas-dust contrast, the trapped dust mass, and the dust contrast at the same orbital location. We apply our model to the recently imaged Oph IRS 48 system, finding values within the range of the observational uncertainties.
C1 [Lyra, Wladimir] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lyra, Wladimir] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Lin, Min-Kai] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
RP Lyra, W (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM wlyra@caltech.edu; mklin924@cita.utoronto.ca
FU National Science Foundation [AST10-09802]; California Institute of
Technology (Caltech); National Aeronautics and Space Administration
(NASA) through the Sagan Fellowship Program; CITA Postdoctoral
Fellowship
FX W.L. acknowledges financial support by the National Science Foundation
under grant No. AST10-09802. This work was performed in part at the Jet
Propulsion Laboratory, under contract with the California Institute of
Technology (Caltech) funded by the National Aeronautics and Space
Administration (NASA) through the Sagan Fellowship Program executed by
the NASA Exoplanet Science Institute. M.K.L. is supported by a CITA
Postdoctoral Fellowship. The authors are indebted to J. Carpenter, A.
Isella, C. McNally, J. Oishi, and L. Ricci for thoughtful suggestions,
and to N. van der Marel for clarifying details concerning the
observations of Oph IRS 48. We also thank the anonymous referee for
questions and comments that helped improve the work.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
AR 17
DI 10.1088/0004-637X/775/1/17
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800017
ER
PT J
AU Miyasaka, H
Bachetti, M
Harrison, FA
Furst, F
Barret, D
Bellm, EC
Boggs, SE
Chakrabarty, D
Chenevez, J
Christensen, FE
Craig, WW
Grefenstette, BW
Hailey, CJ
Madsen, KK
Natalucci, L
Pottschmidt, K
Stern, D
Tomsick, JA
Walton, DJ
Wilms, J
Zhang, W
AF Miyasaka, Hiromasa
Bachetti, Matteo
Harrison, Fiona A.
Fuerst, Felix
Barret, Didier
Bellm, Eric C.
Boggs, Steven E.
Chakrabarty, Deepto
Chenevez, Jerome
Christensen, Finn E.
Craig, William W.
Grefenstette, Brian W.
Hailey, Charles J.
Madsen, Kristin K.
Natalucci, Lorenzo
Pottschmidt, Katja
Stern, Daniel
Tomsick, John A.
Walton, Dominic J.
Wilms, Joern
Zhang, William
TI NuSTAR DETECTION OF HARD X-RAY PHASE LAGS FROM THE ACCRETING PULSAR GS
0834-430
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; pulsars: individual (GS 0834-430); stars: neutron;
X-rays: binaries
ID QUASI-PERIODIC OSCILLATIONS; CYGNUS X-1; MAGNETIC-FIELDS;
TIMING-EXPLORER; TIME-LAGS; MODEL; STAR; COMPTONIZATION; VARIABILITY;
RADIATION
AB The Nuclear Spectroscopic Telescope Array hard X-ray telescope observed the transient Be/X-ray binary GS 0834-430 during its 2012 outburst-the first active state of this system observed in the past 19 yr. We performed timing and spectral analysis and measured the X-ray spectrum between 3-79 keV with high statistical significance. We find the phase-averaged spectrum to be consistent with that observed in many other magnetized, accreting pulsars. We fail to detect cyclotron resonance scattering features that would allow us to constrain the pulsar's magnetic field in either phase-averaged or phase-resolved spectra. Timing analysis shows a clearly detected pulse period of similar to 12.29 s in all energy bands. The pulse profiles show a strong, energy-dependent hard phase lag of up to 0.3 cycles in phase, or about 4 s. Such dramatic energy-dependent lags in the pulse profile have never before been reported in high-mass X-ray binary pulsars. Previously reported lags have been significantly smaller in phase and restricted to low energies (E < 10 keV). We investigate the possible mechanisms that might produce this energy-dependent pulse phase shift. We find the most likely explanation for this effect is a complex beam geometry.
C1 [Miyasaka, Hiromasa; Harrison, Fiona A.; Fuerst, Felix; Bellm, Eric C.; Grefenstette, Brian W.; Madsen, Kristin K.; Walton, Dominic J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Bachetti, Matteo; Barret, Didier] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France.
[Bachetti, Matteo; Barret, Didier] Inst Rech Astrophys & Planetol, CNRS, F-31028 Toulouse 4, France.
[Boggs, Steven E.; Craig, William W.; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Chenevez, Jerome; Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Natalucci, Lorenzo] INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy.
[Pottschmidt, Katja] UMBC, CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, Katja] NASA GSFC, Greenbelt, MD 20771 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wilms, Joern] Dr Karl Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany.
[Zhang, William] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Miyasaka, H (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
EM miyasaka@srl.caltech.edu
RI Wilms, Joern/C-8116-2013; Boggs, Steven/E-4170-2015;
OI Wilms, Joern/0000-0003-2065-5410; Boggs, Steven/0000-0001-9567-4224;
Bachetti, Matteo/0000-0002-4576-9337; Madsen,
Kristin/0000-0003-1252-4891
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; Centre
National d'Etudes Spatiales (CNES); [ASI/INAF I/037/12/0]
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). Matteo Bachetti wishes to acknowledge the
support from the Centre National d'Etudes Spatiales (CNES). Lorenzo
Natalucci acknowledges financial support through contract ASI/INAF
I/037/12/0.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
AR 65
DI 10.1088/0004-637X/775/1/65
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800065
ER
PT J
AU Morley, CV
Fortney, JJ
Kempton, EMR
Marley, MS
Vissher, C
Zahnle, K
AF Morley, Caroline V.
Fortney, Jonathan J.
Kempton, Eliza M. -R.
Marley, Mark S.
Vissher, Channon
Zahnle, Kevin
TI QUANTITATIVELY ASSESSING THE ROLE OF CLOUDS IN THE TRANSMISSION SPECTRUM
OF GJ 1214b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites:
composition; planets and satellites: individual (GJ1214b)
ID HUBBLE-SPACE-TELESCOPE; SUPER-EARTH GJ1214B; TRANSITING PLANET
ATMOSPHERES; COLLISION-INDUCED ABSORPTION; EXTRASOLAR GIANT PLANETS;
DWARF MODEL ATMOSPHERES; EXOPLANET HD 189733B; BROWN DWARFS; ICE CLOUDS;
C/O RATIO
AB Recent observations of the super-Earth GJ 1214b show that it has a relatively featureless transmission spectrum. One suggestion is that these observations indicate that the planet's atmosphere is vertically compact, perhaps due to a water-rich composition that yields a large mean molecular weight. Another suggestion is that the atmosphere is hydrogen/helium-rich with clouds that obscure predicted absorption features. Previous models that incorporate clouds have included their effect without a strong physical motivation for their existence. Here, we present model atmospheres of GJ 1214b that include physically motivated clouds of two types. We model the clouds that are present in chemical equilibrium, as has been suggested to occur on brown dwarfs, which include KCl and ZnS for this planet. We also include clouds that form as a result of photochemistry, forming a hydrocarbon haze layer. We use a photochemical kinetics model to understand the vertical distribution and available mass of haze-forming molecules. We model both solar and enhanced-metallicity cloudy models and determine the cloud properties necessary to match observations. In enhanced-metallicity atmospheres, we find that the equilibrium clouds can match the observations of GJ 1214b if they are lofted high into the atmosphere and have a low sedimentation efficiency (f(sed) = 0.1). We find that models with a variety of hydrocarbon haze properties can match the observations. Particle sizes from 0.01 to 0.25 mu m can match the transmission spectrum with haze-forming efficiencies as low as 1%-5%.
C1 [Morley, Caroline V.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Kempton, Eliza M. -R.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
[Marley, Mark S.; Zahnle, Kevin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Vissher, Channon] SW Res Inst, Boulder, CO 80302 USA.
RP Morley, CV (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
EM cmorley@ucolick.org
RI Marley, Mark/I-4704-2013;
OI Fortney, Jonathan/0000-0002-9843-4354; Marley, Mark/0000-0002-5251-2943
FU NASA [HST-GO-12251.05-A, NNX12AI43A]; NASA PATM [NNX11AD64G]
FX This work benefited from helpful conversations with Jacob Bean and
support from NASA grants HST-GO-12251.05-A and NNX12AI43A. M.S.M.
acknowledges support of NASA PATM program. C.V. acknowledges support
from NASA PATM grant NNX11AD64G.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
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AR 33
DI 10.1088/0004-637X/775/1/33
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800033
ER
PT J
AU Sanchis-Ojeda, R
Winn, JN
Marcy, GW
Howard, AW
Isaacson, H
Johnson, JA
Torres, G
Albrecht, S
Campante, TL
Chaplin, WJ
Davies, GR
Lund, MN
Carter, JA
Dawson, RI
Buchhave, LA
Everett, ME
Fischer, DA
Geary, JC
Gilliland, RL
Horch, EP
Howell, SB
Latham, DW
AF Sanchis-Ojeda, Roberto
Winn, Joshua N.
Marcy, Geoffrey W.
Howard, Andrew W.
Isaacson, Howard
Johnson, John Asher
Torres, Guillermo
Albrecht, Simon
Campante, Tiago L.
Chaplin, William J.
Davies, Guy R.
Lund, Mikkel N.
Carter, Joshua A.
Dawson, Rebekah I.
Buchhave, Lars A.
Everett, Mark E.
Fischer, Debra A.
Geary, John C.
Gilliland, Ronald L.
Horch, Elliott P.
Howell, Steve B.
Latham, David W.
TI KEPLER-63b: A GIANT PLANET IN A POLAR ORBIT AROUND A YOUNG SUN-LIKE STAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: activity; stars: individual (Kepler-63);
stars: rotation; starspots
ID TRANSITING PLANET; EXOPLANETARY SYSTEM; LIGHT-CURVE; INITIAL
CHARACTERISTICS; NEPTUNE HAT-P-11B; STELLAR ROTATION; ERROR-CORRECTION;
RADIAL-VELOCITY; HOT JUPITERS; CADENCE DATA
AB We present the discovery and characterization of a giant planet orbiting the young Sun-like star Kepler-63 (KOI-63, m(Kp) = 11.6, T-eff = 5576 K, M-star = 0.98 M-circle dot). The planet transits every 9.43 days, with apparent depth variations and brightening anomalies caused by large starspots. The planet's radius is 6.1 +/- 0.2 R-circle plus, based on the transit light curve and the estimated stellar parameters. The planet's mass could not be measured with the existing radial-velocity data, due to the high level of stellar activity, but if we assume a circular orbit, then we can place a rough upper bound of 120M(circle plus) (3 sigma). The host star has a high obliquity (Psi= 104 degrees), based on the Rossiter-McLaughlin effect and an analysis of starspot-crossing events. This result is valuable because almost all previous obliquity measurements are for stars with more massive planets and shorter-period orbits. In addition, the polar orbit of the planet combined with an analysis of spot-crossing events reveals a large and persistent polar starspot. Such spots have previously been inferred using Doppler tomography, and predicted in simulations of magnetic activity of young Sun-like stars.
C1 [Sanchis-Ojeda, Roberto; Winn, Joshua N.; Albrecht, Simon] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Sanchis-Ojeda, Roberto; Winn, Joshua N.; Albrecht, Simon] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Johnson, John Asher] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Torres, Guillermo; Carter, Joshua A.; Dawson, Rebekah I.; Geary, John C.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Campante, Tiago L.; Chaplin, William J.; Davies, Guy R.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Lund, Mikkel N.] Aarhus Univ, Stellar Astrophys Ctr SAC, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Gilliland, Ronald L.] Penn State Univ, Davey Lab 525, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Horch, Elliott P.] So Connecticut State Univ, New Haven, CT 06515 USA.
[Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Sanchis-Ojeda, R (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Davies, Guy/0000-0002-4290-7351;
Buchhave, Lars A./0000-0003-1605-5666; Fischer,
Debra/0000-0003-2221-0861
FU NASA's Science Mission Directorate; NASA [NAS5-26555, HF-51267.01-A];
NASA Office of Space Science [NNX09AF08G]; NSF-GRFP [DGE-1144152];
Alfred P. Sloan Foundation; David and Lucile Packard Foundation; UK
Science and Technology Facilities Council (STFC); Danish National
Research Foundation [DNRF106]; ASTERISK project; European Research
Council [267864]; NSF [AST-1007992]
FX We thank the anonymous referee for numerous insightful suggestions that
led to major improvements in this paper. We also thank Andrew Collier
Cameron, Bryce Croll, and Benjamin Brown for helpful discussions, and
the entire Kepler team for the success of the mission. R.S.O. and J.N.W.
acknowledge NASA support through the Kepler Participating Scientist
program. Kepler was competitively selected as the tenth Discovery
mission. Funding for this mission was provided by NASA's Science Mission
Directorate. The data presented in this article 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. J.A.C. acknowledges support by NASA through a
Hubble Fellowship (grant HF-51267.01-A). R.I.D. is supported by the
NSF-GRFP (DGE-1144152). J.A.J. is supported by generous grants from the
Alfred P. Sloan Foundation and the David and Lucile Packard Foundation.
T.L.C., W.J.C., and G.R.D. acknowledge the support of the UK Science and
Technology Facilities Council (STFC). Funding for the Stellar
Astrophysics Centre is provided by The Danish National Research
Foundation (grant agreement DNRF106). This research was partly supported
by the ASTERISK project (ASTERoseismic Investigations with SONG and
Kepler) funded by the European Research Council (grant agreement No.
267864). G.T. acknowledges partial support for this work from NSF grant
AST-1007992.
NR 87
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
AR UNSP 54
DI 10.1088/0004-637X/775/1/54
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800054
ER
PT J
AU Tupa, PR
DeLeo, GG
McCluskey, GE
Kondo, Y
Sahade, J
Gimenez, A
Caton, DB
AF Tupa, Peter R.
DeLeo, Gary G.
McCluskey, George E.
Kondo, Yoji
Sahade, Jorge
Gimenez, Alvaro
Caton, Daniel B.
TI ULTRAVIOLET SPECTROSCOPIC ANALYSIS OF TRANSIENT MASS FLOW OUTBURST IN U
CEPHEI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; binaries: spectroscopic; circumstellar matter;
ultraviolet: stars
ID ALGOL BINARIES; DOPPLER TOMOGRAPHY; SIMULTANEOUS LIGHT; CURVE SOLUTIONS;
ACCRETION; STARS; HOT; ATMOSPHERES; EMISSION; SPECTRA
AB Spectra from the International Ultraviolet Explorer taken in 1989 September over one full orbital period of U Cephei (U Cep, HD 5796) are analyzed. The TLUSTY and SYNSPEC stellar atmospheric simulation programs are used to generate synthetic spectra to which U Cep continuum levels are normalized. Absorption lines attributed to the photosphere are divided out to isolate mass flow and accretion spectra. A radial velocity curve is constructed for conspicuous gas stream features, and shows evidence for a transient flow during secondary eclipse with outward velocities ranging between 200 and 350 km s(-1), and a number density of (3 +/- 2) x 10(10) cm(-3). The validity of C IV 1548 and 1550 and Si IV 1393 and 1402 lines are re-examined in the context of extreme rotational blending effects. A G-star to B-star mass transfer rate of (5 +/- 4) x 10(-9) M-circle dot yr(-1) is calculated as an approximate upper limit, and a model system is presented.
C1 [Tupa, Peter R.; DeLeo, Gary G.; McCluskey, George E.] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA.
[Kondo, Yoji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sahade, Jorge] Fac Ciencias Astron, La Plata, Buenos Aires, Argentina.
[Gimenez, Alvaro] CSIC INTA, Ctr Astrobiol, E-28850 Torrejon De Ardoz, Madrid, Spain.
[Caton, Daniel B.] Appalachian State Univ, Boone, NC 28608 USA.
RP Tupa, PR (reprint author), Lehigh Univ, Dept Phys, Bldg 16, Bethlehem, PA 18015 USA.
EM pet205@lehigh.edu
FU NASA [NAS5-26555]; NASA Office of Space Science [NAG5-7584]
FX All of the IUE 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-HST data is provided by the NASA Office of Space Science via grant
NAG5-7584 and by other grants and contracts.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
DI 10.1088/0004-637X/775/1/46
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800046
ER
PT J
AU Valencia, D
Guillot, T
Parmentier, V
Freedman, RS
AF Valencia, Diana
Guillot, Tristan
Parmentier, Vivien
Freedman, Richard S.
TI BULK COMPOSITION OF GJ 1214b AND OTHER SUB-NEPTUNE EXOPLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE opacity; planets and satellites: composition; planets and satellites:
individual (GJ 1214b, Kepler-11e); planets and satellites: interiors
ID METAL-RICH ATMOSPHERE; SUPER-EARTH GJ1214B; LOW-MASS; TRANSMISSION
SPECTROSCOPY; THERMAL EVOLUTION; GIANT PLANETS; KEPLER-11; SYSTEM;
EQUATION; OPACITIES
AB GJ 1214b stands out among the detected low-mass exoplanets, because it is, so far, the only one amenable to transmission spectroscopy. Up to date there is no consensus about the composition of its envelope although most studies suggest a high molecular weight atmosphere. In particular, it is unclear if hydrogen and helium are present or if the atmosphere is water dominated. Here, we present results on the composition of the envelope obtained by using an internal structure and evolutionary model to fit the mass and radius data. By examining all possible mixtures of water and H/He, with the corresponding opacities, we find that the bulk amount of H/He of GJ 1214b is at most 7% by mass. In general, we find the radius of warm sub-Neptunes to be most sensitive to the amount of H/He. We note that all (Kepler-11b, c, d, f, Kepler-18b, Kepler-20b, 55Cnc-e, Kepler-36c, and Kepler-68b) but two (Kepler-11e and Kepler-30b) of the discovered low-mass planets so far have less than 10% H/He. In fact, Kepler-11e and Kepler-30b have 10%-18% and 5%-15% bulk H/He. Conversely, little can be determined about the H2O or rocky content of sub-Neptune planets. We find that although a 100% water composition fits the data for GJ 1214b, based on formation constraints the presence of heavier refractory material on this planet is expected, and hence, so is a component lighter than water required. The same is true for Kepler-11f. A robust determination by transmission spectroscopy of the composition of the upper atmosphere of GJ 1214b will help determine the extent of compositional segregation between the atmosphere and the envelope.
C1 [Valencia, Diana] MIT, Earth Atmosphere & Planetary Sci Dept, Cambridge, MA 02139 USA.
[Guillot, Tristan; Parmentier, Vivien] Univ Nice Sophie Antipolis, CNRS, Observ Cote Azur, UMR 7293, F-06300 Nice 4, France.
[Freedman, Richard S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Freedman, Richard S.] Seti Inst, Mountain View, CA 94043 USA.
RP Valencia, D (reprint author), MIT, Earth Atmosphere & Planetary Sci Dept, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM dianav@mit.edu
FU California Institute of Technology (Caltech); NASA
FX 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. We
thank Ignasi Ribas for his comments on the XUV fluxes of stars. We thank
Jonathan Fortney for his careful and insightful review that has
significantly increased the quality of the manuscript.
NR 38
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2013
VL 775
IS 1
AR 10
DI 10.1088/0004-637X/775/1/10
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 220VU
UT WOS:000324615800010
ER
PT J
AU Alexander, CE
Walsh, RW
Regnier, S
Cirtain, J
Winebarger, AR
Golub, L
Kobayashi, K
Platt, S
Mitchell, N
Korreck, K
DePontieu, B
DeForest, C
Weber, M
Title, A
Kuzin, S
AF Alexander, Caroline E.
Walsh, Robert W.
Regnier, Stephane
Cirtain, Jonathan
Winebarger, Amy R.
Golub, Leon
Kobayashi, Ken
Platt, Simon
Mitchell, Nick
Korreck, Kelly
DePontieu, Bart
DeForest, Craig
Weber, Mark
Title, Alan
Kuzin, Sergey
TI ANTI-PARALLEL EUV FLOWS OBSERVED ALONG ACTIVE REGION FILAMENT THREADS
WITH HI-C
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: corona; Sun: filaments, prominences
ID SOLAR PROMINENCES; HINODE; ALPHA; LOOPS; MOSS; AIA
AB Plasma flows within prominences/filaments have been observed for many years and hold valuable clues concerning the mass and energy balance within these structures. Previous observations of these flows primarily come from Ha and cool extreme-ultraviolet (EUV) lines (e. g., 304 angstrom) where estimates of the size of the prominence threads has been limited by the resolution of the available instrumentation. Evidence of "counter-steaming" flows has previously been inferred from these cool plasma observations, but now, for the first time, these flows have been directly imaged along fundamental filament threads within the million degree corona (at 193 angstrom). In this work, we present observations of an AR filament observed with the High-resolution Coronal Imager (Hi-C) that exhibits anti-parallel flows along adjacent filament threads. Complementary data from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager are presented. The ultra-high spatial and temporal resolution of Hi-C allow the anti-parallel flow velocities to be measured (70-80 km s(-1)) and gives an indication of the resolvable thickness of the individual strands (0 ''.8 +/- 0 ''.1). The temperature of the plasma flows was estimated to be log T (K) = 5.45 +/- 0.10 using Emission Measure loci analysis. We find that SDO/AIA cannot clearly observe these anti-parallel flows or measure their velocity or thread width due to its larger pixel size. We suggest that anti-parallel/counter-streaming flows are likely commonplace within all filaments and are currently not observed in EUV due to current instrument spatial resolution.
C1 [Alexander, Caroline E.; Walsh, Robert W.; Regnier, Stephane] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Cirtain, Jonathan; Winebarger, Amy R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Golub, Leon; Korreck, Kelly; Weber, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kobayashi, Ken] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA.
[Platt, Simon; Mitchell, Nick] Univ Cent Lancashire, Sch Comp Engn & Phys Sci, Preston PR1 2HE, Lancs, England.
[DePontieu, Bart; Title, Alan] Org ADBS, Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA USA.
[DeForest, Craig] SW Res Inst, Boulder, CO 80302 USA.
[Kuzin, Sergey] Russian Acad Sci, PN Lebedev Phys Inst, Moscow 119991, Russia.
RP Alexander, CE (reprint author), Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
RI Regnier, Stephane/H-9107-2012; Platt, Simon/C-6048-2008; Kuzin,
Sergey/M-3435-2015; Regnier, Stephane/K-2423-2015
OI Regnier, Stephane/0000-0001-8954-4183; Platt, Simon/0000-0003-4431-8814;
Regnier, Stephane/0000-0001-8954-4183
NR 25
TC 18
Z9 18
U1 1
U2 5
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 SEP 20
PY 2013
VL 775
IS 1
AR L32
DI 10.1088/2041-8205/775/1/L32
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 217ET
UT WOS:000324340500032
ER
PT J
AU Cao, Y
Kasliwal, MM
Arcavi, I
Horesh, A
Hancock, P
Valenti, S
Cenko, SB
Kulkarni, SR
Gal-Yam, A
Gorbikov, E
Ofek, EO
Sand, D
Yaron, O
Graham, M
Silverman, JM
Wheeler, JC
Marion, GH
Walker, ES
Mazzali, P
Howell, DA
Li, KL
Kong, AKH
Bloom, JS
Nugent, PE
Surace, J
Masci, F
Carpenter, J
Degenaar, N
Gelino, CR
AF Cao, Yi
Kasliwal, Mansi M.
Arcavi, Iair
Horesh, Assaf
Hancock, Paul
Valenti, Stefano
Cenko, S. Bradley
Kulkarni, S. R.
Gal-Yam, Avishay
Gorbikov, Evgeny
Ofek, Eran O.
Sand, David
Yaron, Ofer
Graham, Melissa
Silverman, Jeffrey M.
Wheeler, J. Craig
Marion, G. H.
Walker, Emma S.
Mazzali, Paolo
Howell, D. Andrew
Li, K. L.
Kong, A. K. H.
Bloom, Joshua S.
Nugent, Peter E.
Surace, Jason
Masci, Frank
Carpenter, John
Degenaar, Nathalie
Gelino, Christopher R.
TI DISCOVERY, PROGENITOR AND EARLY EVOLUTION OF A STRIPPED ENVELOPE
SUPERNOVA iPTF13bvn
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE instrumentation: adaptive optics; shock waves; stars: Wolf-Rayet;
supernovae: individual (iPTF13bvn); surveys
ID CORE-COLLAPSE SUPERNOVA; X-RAY; ECHELLE SPECTROMETER; IC SUPERNOVAE;
LIGHT CURVES; TELESCOPE; RADIO; STAR; SPECTROGRAPH; ABSORPTION
AB The intermediate Palomar Transient Factory reports our discovery of a young supernova, iPTF13bvn, in the nearby galaxy, NGC 5806 (22.5 Mpc). Our spectral sequence in the optical and infrared suggests a Type Ib classification. We identify a blue progenitor candidate in deep pre-explosion imaging within a 2 sigma error circle of 80 mas (8.7 pc). The candidate has an M-B luminosity of -5.52 +/- 0.39 mag and a B-I color of 0.25 +/- 0.25 mag. If confirmed by future observations, this would be the first direct detection for a progenitor of a Type Ib. Fitting a power law to the early light curve, we find an extrapolated explosion date around 0.6 days before our first detection. We see no evidence of shock cooling. The pre-explosion detection limits constrain the radius of the progenitor to be smaller than a few solar radii. iPTF13bvn is also detected in centimeter and millimeter wavelengths. Fitting a synchrotron self-absorption model to our radio data, we find a mass-loading parameter of 1.3x10(12) g cm(-1). Assuming a wind velocity of 10(3) km s(-1), we derive a progenitor mass-loss rate of 3 x 10(-5) M-circle dot yr(-1). Our observations, taken as a whole, are consistent with a Wolf-Rayet progenitor of the supernova iPTF13bvn.
C1 [Cao, Yi; Horesh, Assaf; Kulkarni, S. R.; Carpenter, John] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Kasliwal, Mansi M.] Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Arcavi, Iair; Gal-Yam, Avishay; Gorbikov, Evgeny; Ofek, Eran O.; Yaron, Ofer] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Hancock, Paul] Univ Sydney, Sydney Inst Astron SIfA, Sch Phys, Sydney, NSW 2006, Australia.
[Hancock, Paul] Univ Sydney, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia.
[Valenti, Stefano; Graham, Melissa; Howell, D. Andrew] Global Telescope Network, Las Cumbres Observ, Goleta, CA 93117 USA.
[Valenti, Stefano; Graham, Melissa; Howell, D. Andrew; Nugent, Peter E.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Cenko, S. Bradley] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sand, David] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
[Silverman, Jeffrey M.; Wheeler, J. Craig; Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Walker, Emma S.] Yale Univ, Dept Phys, New Haven, CT 06511 USA.
[Mazzali, Paolo] INAF Padova Astron Observ, I-35122 Padua, Italy.
[Mazzali, Paolo] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5UX, Merseyside, England.
[Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Li, K. L.; Kong, A. K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan.
[Li, K. L.; Kong, A. K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan.
[Bloom, Joshua S.; Nugent, Peter E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Computat Res Div, Berkeley, CA 94720 USA.
[Surace, Jason] CALTECH, Spitzer Sci Ctr, Jet Prop Lab, Pasadena, CA 91125 USA.
[Masci, Frank; Gelino, Christopher R.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Degenaar, Nathalie] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
RP Cao, Y (reprint author), CALTECH, Dept Astron, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM ycao@astro.caltech.edu
RI Horesh, Assaf/O-9873-2016
OI Horesh, Assaf/0000-0002-5936-1156
FU Hubble Fellowship; Carnegie-Princeton Fellowship; NSF [AST-1302771, AST
11-09801]; ISF; BSF; GIF; Minerva; EU/FP7 via an ERC; Kimmel award;
Office of Science of the U.S. Department of Energy; Commonwealth of
Australia; Australian Research Council [FS100100033]; National Science
Foundation; CARMA partner universities; [CE110001020]
FX M.M.K. acknowledges generous support from the Hubble Fellowship and
Carnegie-Princeton Fellowship. J.M.S. is supported by an NSF Astronomy
and Astrophysics Postdoctoral Fellowship under award AST-1302771. N.D.
acknowledges the Hubble Fellowship. Research by A.G.Y. and his group was
supported by grants from the ISF, BSF, GIF, Minerva, the EU/FP7 via an
ERC grant and the Kimmel award. The research of J.C.W. is supported by
NSF Grant AST 11-09801.; The National Energy Research Scientific
Computing Center, supported by the Office of Science of the U.S.
Department of Energy, provided staff, computational resources, and data
storage for this project. The Australia Telescope is funded by the
Commonwealth of Australia for operation as a National Facility managed
by CSIRO. This research has been supported by the Australian Research
Council through Super Science Fellowship grant FS100100033. The Centre
for All-sky Astrophysics is an Australian Research Council Centre of
Excellence, funded by grant CE110001020. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. Ongoing
CARMA development and operations are supported by the National Science
Foundation under a cooperative agreement, and by the CARMA partner
universities.
NR 49
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2013
VL 775
IS 1
AR L7
DI 10.1088/2041-8205/775/1/L7
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 217ET
UT WOS:000324340500007
ER
PT J
AU Dowell, J
Ray, PS
Taylor, GB
Blythe, JN
Clarke, T
Craig, J
Ellingson, SW
Helmboldt, JF
Henning, PA
Lazio, TJW
Schinzel, F
Stovall, K
Wolfe, CN
AF Dowell, J.
Ray, P. S.
Taylor, G. B.
Blythe, J. N.
Clarke, T.
Craig, J.
Ellingson, S. W.
Helmboldt, J. F.
Henning, P. A.
Lazio, T. J. W.
Schinzel, F.
Stovall, K.
Wolfe, C. N.
TI DETECTION AND FLUX DENSITY MEASUREMENTS OF THE MILLISECOND PULSAR
J2145-0750 BELOW 100 MHz
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE pulsars: general; pulsars: individual (PSR J2145-0750)
ID SCINTILLATION; DISPERSION; TELESCOPE; SPECTRA
AB We present flux density measurements and pulse profiles for the millisecond pulsar PSR J2145-0750 spanning 37 to 81 MHz using data obtained from the first station of the Long Wavelength Array. These measurements represent the lowest frequency detection of pulsed emission from a millisecond pulsar to date. We find that the pulse profile is similar to that observed at 102 MHz. We also find that the flux density spectrum between approximate to 40 MHz to 5 GHz is suggestive of a break and may be better fit by a model that includes spectral curvature with a rollover around 730 MHz rather than a single power law.
C1 [Dowell, J.; Taylor, G. B.; Craig, J.; Henning, P. A.; Schinzel, F.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
[Ray, P. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Blythe, J. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA USA.
[Clarke, T.; Helmboldt, J. F.] US Naval Res Lab, Washington, DC 20375 USA.
[Ellingson, S. W.; Wolfe, C. N.] Virginia Tech, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24061 USA.
[Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stovall, K.] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA.
[Stovall, K.] Univ Texas Brownsville, Dept Phys & Astron, Brownsville, TX 78520 USA.
RP Dowell, J (reprint author), Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
EM jdowell@unm.edu
RI Stovall, Kevin/D-9844-2014; Helmboldt, Joseph/C-8105-2012;
OI Stovall, Kevin/0000-0002-7261-594X; Ray, Paul/0000-0002-5297-5278
FU Office of Naval Research [N00014-07-C-0147]; National Science Foundation
[AST-1139963, AST-1139974]
FX We thank the anonymous referee for thoughtful comments. Construction of
the LWA has been supported by the Office of Naval Research under
Contract N00014-07-C-0147. Support for operations and continuing
development of LWA1 is provided by the National Science Foundation under
grants AST-1139963 and AST-1139974 of the University Radio Observatories
program. 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 19
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2013
VL 775
IS 1
AR L28
DI 10.1088/2041-8205/775/1/L28
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 217ET
UT WOS:000324340500028
ER
PT J
AU Hashimoto, J
Dong, R
Kudo, T
Honda, M
McClure, MK
Zhu, Z
Muto, T
Wisniewski, J
Abe, L
Brandner, W
Brandt, T
Carson, J
Egner, S
Feldt, M
Fukagawa, M
Goto, M
Grady, CA
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, K
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, G
Kusakabe, N
Kuzuhara, M
Kwon, J
Matsuo, T
Mayama, S
McElwain, MW
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, G
Suenaga, T
Suto, H
Suzuki, R
Takahashi, Y
Takami, M
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Hashimoto, J.
Dong, R.
Kudo, T.
Honda, M.
McClure, M. K.
Zhu, Z.
Muto, T.
Wisniewski, J.
Abe, L.
Brandner, W.
Brandt, T.
Carson, J.
Egner, S.
Feldt, M.
Fukagawa, M.
Goto, M.
Grady, C. A.
Guyon, O.
Hayano, Y.
Hayashi, M.
Hayashi, S.
Henning, T.
Hodapp, K.
Ishii, M.
Iye, M.
Janson, M.
Kandori, R.
Knapp, G.
Kusakabe, N.
Kuzuhara, M.
Kwon, J.
Matsuo, T.
Mayama, S.
McElwain, M. W.
Miyama, S.
Morino, J. -I.
Moro-Martin, A.
Nishimura, T.
Pyo, T. -S.
Serabyn, G.
Suenaga, T.
Suto, H.
Suzuki, R.
Takahashi, Y.
Takami, M.
Takato, N.
Terada, H.
Thalmann, C.
Tomono, D.
Turner, E. L.
Watanabe, M.
Yamada, T.
Takami, H.
Usuda, T.
Tamura, M.
TI POLARIMETRIC IMAGING OF LARGE CAVITY STRUCTURES IN THE PRE-TRANSITIONAL
PROTOPLANETARY DISK AROUND PDS 70: OBSERVATIONS OF THE DISK (vol 758,
L19, 2012)
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Correction
C1 [Hashimoto, J.; Wisniewski, J.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Dong, R.; Zhu, Z.; Brandt, T.; Janson, M.; Knapp, G.; Moro-Martin, A.; Turner, E. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kudo, T.; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Ishii, M.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.; Takami, H.; Usuda, T.] Subaru Telescope, Hilo, HI 96720 USA.
[Honda, M.] Kanagawa Univ, Hiratsuka, Kanagawa 2591293, Japan.
[McClure, M. K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Muto, T.] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan.
[Abe, L.] Univ Nice Sophia Antipolis, Lab Hippolyte Fizeau, UMR6525, F-06108 Nice 2, France.
[Brandner, W.; Feldt, M.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Fukagawa, M.] Osaka Univ, Toyonaka, Osaka 5600043, Japan.
[Goto, M.] Univ Sternwarte, D-81679 Munich, Germany.
[Grady, C. A.; McElwain, M. W.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Grady, C. A.] Eureka Sci, Oakland, CA 96002 USA.
[Hayashi, M.; Iye, M.; Kandori, R.; Kusakabe, N.; Kuzuhara, M.; Kwon, J.; Morino, J. -I.; Suenaga, T.; Suto, H.; Suzuki, R.; Takahashi, Y.; Tamura, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Hodapp, K.] Univ Hawaii, Hilo, HI 96720 USA.
[Kuzuhara, M.] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan.
[Kuzuhara, M.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Kwon, J.; Suenaga, T.] Grad Univ Adv Studies Sokendai, Dept Astron Sci, Tokyo 1818588, Japan.
[Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Mayama, S.] Grad Univ Adv Studies, Shonan Int Village, Miura, Kanagawa 2400193, Japan.
[Miyama, S.] Hiroshima Univ, Higashihiroshima 7398511, Japan.
[Moro-Martin, A.] CAB CSIC INTA, Dept Astrophys, E-28850 Torrejon De Ardoz, Madrid, Spain.
[Serabyn, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Takahashi, Y.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Turner, E. L.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2278568, Japan.
[Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan.
[Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Hashimoto, J (reprint author), Univ Oklahoma, HL Dodge Dept Phys & Astron, 440 West Brooks St, Norman, OK 73019 USA.
EM jun.hashimoto@ou.edu
RI MIYAMA, Shoken/A-3598-2015
NR 1
TC 1
Z9 1
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2013
VL 775
IS 1
AR L33
DI 10.1088/2041-8205/775/1/L33
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 217ET
UT WOS:000324340500033
ER
PT J
AU Wang, TJ
Ofman, L
Davila, JM
AF Wang, Tongjiang
Ofman, Leon
Davila, Joseph M.
TI THREE-DIMENSIONAL MAGNETOHYDRODYNAMIC MODELING OF PROPAGATING
DISTURBANCES IN FAN-LIKE CORONAL LOOPS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE magnetohydrodynamics (MHD); Sun: activity; Sun: corona; Sun:
oscillations; Sun: UV radiation; waves
ID SLOW MAGNETOSONIC WAVES; ACTIVE-REGION LOOPS; SPECTROSCOPIC
OBSERVATIONS; MAGNETOACOUSTIC WAVES; SOLAR-WIND; OSCILLATIONS; OUTFLOWS;
BRIGHTENINGS; HINODE; TRACE
AB Quasi-periodic propagating intensity disturbances (PDs) have been observed in large coronal loops in EUV images over a decade, and are widely accepted to be slow magnetosonic waves. However, spectroscopic observations from Hinode/EIS revealed their association with persistent coronal upflows, making this interpretation debatable. Motivated by the scenario that the coronal upflows could be the cumulative result of numerous individual flow pulses generated by sporadic heating events (nanoflares) at the loop base, we construct a velocity driver with repetitive tiny pulses, whose energy frequency distribution follows the flare power-law scaling. We then perform three-dimensional MHD modeling of an idealized bipolar active region by applying this broadband velocity driver at the footpoints of large coronal loops which appear open in the computational domain. Our model successfully reproduces the PDs with similar features as the observed, and shows that any upflow pulses inevitably excite slow magnetosonic wave disturbances propagating along the loop. We find that the generated PDs are dominated by the wave signature as their propagation speeds are consistent with the wave speed in the presence of flows, and the injected flows rapidly decelerate with height. Our simulation results suggest that the observed PDs and associated persistent upflows may be produced by small-scale impulsive heating events (nanoflares) at the loop base in the corona, and that the flows and waves may both contribute to the PDs at lower heights.
C1 [Wang, Tongjiang; Ofman, Leon] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wang, Tongjiang; Ofman, Leon; Davila, Joseph M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Wang, TJ (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave NE, Washington, DC 20064 USA.
EM tongjiang.wang@nasa.gov
FU NASA [NNX12AB34G, NNG11PL10A, NNX11AO68G]
FX The work of T.W. was supported by NASA grant NNX12AB34G and the NASA
Cooperative Agreement NNG11PL10A to CUA. L.O. acknowledges support by
NASA grants NNX12AB34G and NNX11AO68G. We acknowledge the use of
computer resources operated by the NASA Advanced Supercomputing (NAS)
Division at NASA Ames Research Center.
NR 37
TC 22
Z9 23
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2013
VL 775
IS 1
AR L23
DI 10.1088/2041-8205/775/1/L23
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 217ET
UT WOS:000324340500023
ER
PT J
AU Painter, TH
Flanner, MG
Kaser, G
Marzeion, B
VanCuren, RA
Abdalati, W
AF Painter, Thomas H.
Flanner, Mark G.
Kaser, Georg
Marzeion, Ben
VanCuren, Richard A.
Abdalati, Waleed
TI End of the Little Ice Age in the Alps forced by industrial black carbon
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE aerosol; cryosphere; albedo; climate
ID MASS-BALANCE; EUROPEAN ALPS; GLACIER FLUCTUATIONS; RECONSTRUCTION;
VARIABILITY; SWITZERLAND; RECORD; SNOW; HINTEREISFERNER; POLLUTION
AB Glaciers in the European Alps began to retreat abruptly from their mid-19th century maximum, marking what appeared to be the end of the Little Ice Age. Alpine temperature and precipitation records suggest that glaciers should instead have continued to grow until circa 1910. Radiative forcing by increasing deposition of industrial black carbon to snow may represent the driver of the abrupt glacier retreats in the Alps that began in the mid-19th century. Ice cores indicate that black carbon concentrations increased abruptly in the mid-19th century and largely continued to increase into the 20th century, consistent with known increases in black carbon emissions from the industrialization of Western Europe. Inferred annual surface radiative forcings increased stepwise to 13-17 W.m(-2) between 1850 and 1880, and to 9-22 W.m(-2) in the early 1900s, with snowmelt season (April/May/June) forcings reaching greater than 35 W.m(-2) by the early 1900s. These snowmelt season radiative forcings would have resulted in additional annual snow melting of as much as 0.9 m water equivalent across the melt season. Simulations of glacier mass balances with radiative forcing-equivalent changes in atmospheric temperatures result in conservative estimates of accumulating negative mass balances of magnitude -15 m water equivalent by 1900 and -30 m water equivalent by 1930, magnitudes and timing consistent with the observed retreat. These results suggest a possible physical explanation for the abrupt retreat of glaciers in the Alps in the mid-19th century that is consistent with existing temperature and precipitation records and reconstructions.
C1 [Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Flanner, Mark G.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Kaser, Georg; Marzeion, Ben] Univ Innsbruck, Inst Meteorol & Geophys, A-6020 Innsbruck, Austria.
[VanCuren, Richard A.] Univ Calif Davis, Air Qual Res Ctr, Davis, CA 95616 USA.
[Abdalati, Waleed] Cooperat Inst Res Environm Sci, Earth Sci & Observat Ctr, Boulder, CO 80309 USA.
RP Painter, TH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Thomas.Painter@jpl.nasa.gov
RI Flanner, Mark/C-6139-2011; Painter, Thomas/B-7806-2016; Marzeion,
Ben/G-6514-2013
OI Flanner, Mark/0000-0003-4012-174X; Marzeion, Ben/0000-0002-6185-3539
FU National Science Foundation [ATM-0432327, ATM-0852775]; National
Aeronautics and Space Administration [NNX10AO97G]; Austrian Science Fund
(FWF) [P22443-N21]
FX We thank Johannes Oerlemans and Florian Thevenon for access to data.
Part of this work was performed at the Jet Propulsion Laboratory,
California Institute of Technology under a contract with the National
Aeronautics and Space Administration. This research was funded by
National Science Foundation Grant ATM-0432327 (to T. H. P.); National
Aeronautics and Space Administration Project NNX10AO97G (to T. H. P.);
National Science Foundation Grant ATM-0852775 (to M. G. F.); and
Austrian Science Fund (FWF): P22443-N21 (to B.M.).
NR 48
TC 33
Z9 35
U1 3
U2 64
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 SEP 17
PY 2013
VL 110
IS 38
BP 15216
EP 15221
DI 10.1073/pnas.1302570110
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 219GW
UT WOS:000324495300030
PM 24003138
ER
PT J
AU Bauschlicher, CW
Ricca, A
AF Bauschlicher, Charles W.
Ricca, Alessandra
TI Naphthalene dimer and naphthalene dimer with Ar: calibration
calculations and the effect of Ar on the stability and vibrational
frequencies
SO THEORETICAL CHEMISTRY ACCOUNTS
LA English
DT Article
DE Naphthalene dimer; DFT; Dispersion; Infrared spectra
ID POLYCYCLIC AROMATIC-HYDROCARBONS; GAUSSIAN-BASIS SETS;
INFRARED-SPECTROSCOPY; SPECTRA
AB The harmonic vibrational frequencies of naphthalene and its dimers are computed using density functional theory including an empirical correction for dispersion. The C-H out-of-plane bending modes in the naphthalene dimers show a red or a blue shift depending on the relative orientation of the two naphthalene molecules. The addition of Ar atoms does not significantly affect the vibrational frequencies, but changes the energy separation between the two dimer conformations.
C1 [Bauschlicher, Charles W.] NASA, Ames Res Ctr, Entry Syst & Technol Div, Moffett Field, CA 94035 USA.
[Ricca, Alessandra] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
RP Bauschlicher, CW (reprint author), NASA, Ames Res Ctr, Entry Syst & Technol Div, Mail Stop 230-3, Moffett Field, CA 94035 USA.
EM Charles.W.Bauschlicher@nasa.gov; Alessandra.Ricca-1@nasa.gov
FU NASA's Astrophysics Theory and Fundamental Physics (ATFP) [NNX09AD18G];
Laboratory Astrophysics 'Carbon in the Galaxy' Consortium Grant
[NNH10ZDA001N]
FX A.R. thanks the NASA's Astrophysics Theory and Fundamental Physics
(ATFP) (NNX09AD18G) and Laboratory Astrophysics 'Carbon in the Galaxy'
Consortium Grant (NNH10ZDA001N) programs for their generous support of
this work.
NR 18
TC 1
Z9 1
U1 1
U2 10
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1432-881X
J9 THEOR CHEM ACC
JI Theor. Chem. Acc.
PD SEP 17
PY 2013
VL 132
IS 11
AR UNSP 1395
DI 10.1007/s00214-013-1395-z
PG 8
WC Chemistry, Physical
SC Chemistry
GA 227KB
UT WOS:000325110500001
ER
PT J
AU Painter, TH
Seidel, FC
Bryant, AC
Skiles, SM
Rittger, K
AF Painter, Thomas H.
Seidel, Felix C.
Bryant, Ann C.
Skiles, S. McKenzie
Rittger, Karl
TI Imaging spectroscopy of albedo and radiative forcing by light-absorbing
impurities in mountain snow
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE snow; light absorbing impurities; radiative forcing; imaging
spectroscopy; albedo
ID GRAIN-SIZE; COVERED AREA; BLACK CARBON; CLIMATE; REFLECTANCE;
GONIOMETER; RETRIEVAL; MONSOON; RECORD
AB Recent studies show that deposition of dust and black carbon to snow and ice accelerates snowmelt and perturbs regional climate and hydrologic cycles. Radiative forcing by aerosols is often neglected in climate and hydrological models in part due to scarcity of observations. Here we describe and validate an algorithm suite (Imaging Spectrometer-Snow Albedo and Radiative Forcing (IS-SnARF)) that provides quantitative retrievals of snow grain size, snow albedo, and radiative forcing by light-absorbing impurities in snow and ice (LAISI) from Airborne Visible/Infrared Imaging Spectrometer (AVIRIS) data collected on 15 June 2011 in the Senator Beck Basin Study Area (SBBSA), SW Colorado, USA. Radiative forcing by LAISI is retrieved by the integral of the convolution of spectral irradiance with spectral differences between the spectral albedo (scaled from the observed hemispherical-directional reflectance factor (HDRF)) and modeled clean snow spectral albedo. The modeled surface irradiance at time of acquisition at test sites was 1052 W m(-2) compared to 1048 W m(-2) measured with the field spectroradiometer measurements, a relative difference of 0.4%. HDRF retrievals at snow and bare soil sites had mean errors relative to in situ measurements of -0.4 +/- 0.1% reflectance averaged across the spectrum and root-mean-square errors of 1.5 +/- 0.1%. Comparisons of snow albedo and radiative forcing retrievals from AVIRIS with in situ measurements in SBBSA showed errors of 0.001-0.004 and 2.1 +/- 5.1 W m(-2), respectively. A counterintuitive result was that, in the presence of light absorbing impurities, near-surface snow grain size increased with elevation, whereas we generally expect that at lower elevation the grain size would be larger.
C1 [Painter, Thomas H.; Seidel, Felix C.; Rittger, Karl] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Painter, Thomas H.; Skiles, S. McKenzie] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Bryant, Ann C.] Univ Utah, Dept Geog, Salt Lake City, UT USA.
RP Painter, TH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM thomas.painter@jpl.nasa.gov
RI Painter, Thomas/B-7806-2016;
OI Seidel, Felix/0000-0002-4282-2198
FU National Science Foundation [ATM04323237]; NASA [NNX10AO97G]
FX This work was funded by the National Science Foundation grant
ATM04323237 and NASA project NNX10AO97G. Part of this work was performed
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with NASA.
NR 42
TC 18
Z9 18
U1 3
U2 34
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 SEP 16
PY 2013
VL 118
IS 17
BP 9511
EP 9523
DI 10.1002/jgrd.50520
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 232JH
UT WOS:000325489300016
ER
PT J
AU Garfinkel, CI
Waugh, DW
Oman, LD
Wang, L
Hurwitz, MM
AF Garfinkel, C. I.
Waugh, D. W.
Oman, L. D.
Wang, L.
Hurwitz, M. M.
TI Temperature trends in the tropical upper troposphere and lower
stratosphere: Connections with sea surface temperatures and implications
for water vapor and ozone
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE TTL; stratospheric ozone; stratospheric water vapor; stratospheric
temperature trends; SST trends
ID TROPOPAUSE TEMPERATURES; SATELLITE MEASUREMENTS; CLIMATE-CHANGE; MSU;
CIRCULATION; LAYER; ENSO; VARIABILITY; SIMULATION; MODELS
AB Satellite observations and chemistry-climate model experiments are used to understand the zonal structure of tropical lower stratospheric temperature, water vapor, and ozone trends. The warming in the tropical upper troposphere over the past 30 years is strongest near the Indo-Pacific warm pool, while the warming trend in the western and central Pacific is much weaker. In the lower stratosphere, these trends are reversed: the historical cooling trend is strongest over the Indo-Pacific warm pool and is weakest in the western and central Pacific. These zonal variations are stronger than the zonal-mean response in boreal winter. Targeted experiments with a chemistry-climate model are used to demonstrate that sea surface temperature (hereafter SST) trends are driving the zonal asymmetry in upper tropospheric and lower stratospheric tropical temperature trends. Warming SSTs in the Indian Ocean and in the warm pool region have led to enhanced moist heating in the upper troposphere, and in turn to a Gill-like response that extends into the lower stratosphere. The anomalous circulation has led to zonal structure in the ozone and water vapor trends near the tropopause, and subsequently to less water vapor entering the stratosphere. The radiative impact of these changes in trace gases is smaller than the direct impact of the moist heating. Projected future SSTs appear to drive a temperature and water vapor response whose zonal structure is similar to the historical response. In the lower stratosphere, the changes in water vapor and temperature due to projected future SSTs are of similar strength to, though slightly weaker than, that due directly to projected future CO2, ozone, and methane.
C1 [Garfinkel, C. I.; Waugh, D. W.; Wang, L.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Garfinkel, C. I.] Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel.
[Oman, L. D.; Hurwitz, M. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hurwitz, M. M.] Morgan State Univ, Goddard Earth Sci Technol & Res GESTAR, Baltimore, MD 21239 USA.
RP Garfinkel, CI (reprint author), Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel.
EM chaim.garfinkel@mail.huji.ac.il
RI Oman, Luke/C-2778-2009; Wang, Lei/F-1269-2015; garfinkel,
chaim/H-6215-2012; Waugh, Darryn/K-3688-2016
OI Oman, Luke/0000-0002-5487-2598; Wang, Lei/0000-0002-1618-1796;
garfinkel, chaim/0000-0001-7258-666X; Waugh, Darryn/0000-0001-7692-2798
FU NSF [AGS-1036858, ATM-0905863]
FX This work was supported by NSF grants AGS-1036858 and ATM-0905863. We
acknowledge the very helpful feedback from George Kiladis, Karen
Rosenlof, and two anonymous reviewers.
NR 61
TC 14
Z9 14
U1 3
U2 22
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 SEP 16
PY 2013
VL 118
IS 17
BP 9658
EP 9672
DI 10.1002/jgrd.50772
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 232JH
UT WOS:000325489300027
ER
PT J
AU Zhou, YP
Lau, WKM
Liu, CT
AF Zhou, Yaping
Lau, William K. M.
Liu, Chuntao
TI Rain characteristics and large-scale environments of precipitation
objects with extreme rain volumes from TRMM observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE extreme rainfall; large-scale environment; rain characteristics; TRMM
ID CONVECTIVE CLOUD OBJECTS; TYPHOON MORAKOT 2009; LIVED SQUALL LINES; 1998
EL-NINO; FLASH-FLOOD; TROPICAL RAINFALL; DIURNAL CYCLE; INTENSE
PRECIPITATION; STATISTICAL-ANALYSES; PROFILING ALGORITHM
AB This study adopts a precipitation object approach by using 14years of Tropical Rainfall Measuring Mission (TRMM) Precipitation Feature (PF) and National Centers for Environmental Prediction (NCEP) reanalysis data to study rainfall structure and environmental factors associated with extreme heavy rain events. Characteristics of instantaneous extreme volumetric PFs are examined and compared to those of intermediate and small systems. It is found that instantaneous PFs exhibit a much wider scale range compared to the daily gridded precipitation accumulation range. The top 1% of the rainiest PFs contribute over 55% of total rainfall and have 2 orders of rain volume magnitude greater than those of the median PFs. We find a threshold near the top 10% beyond which the PFs grow exponentially into larger, deeper, and colder rain systems. NCEP reanalyses show that midlevel relative humidity and total precipitable water increase steadily with increasingly larger PFs, along with a rapid increase of 500hPa upward vertical velocity beyond the top 10%. This provides the necessary moisture convergence to amplify and sustain the extreme events. The rapid increase in vertical motion is associated with the release of convective available potential energy (CAPE) in mature systems, as is evident in the increase in CAPE of PFs up to 10% and the subsequent dropoff. The study illustrates distinct stages in the development of an extreme rainfall event including (1) a systematic buildup in large-scale temperature and moisture, (2) a rapid change in rain structure, (3) explosive growth of the PF size, and (4) a release of CAPE before the demise of the event.
C1 [Zhou, Yaping] Morgan State Univ, GESTAR, Greenbelt, MD 20771 USA.
[Lau, William K. M.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Liu, Chuntao] Texas A&M Univ, Dept Phys & Environm Sci, Corpus Christi, TX USA.
RP Zhou, YP (reprint author), Morgan State Univ, GESTAR, Greenbelt, MD 20771 USA.
EM yaping.zhou-1@nasa.gov
RI Lau, William /E-1510-2012
OI Lau, William /0000-0002-3587-3691
FU Precipitation Measuring Mission, NASA Earth Science Division
[NNX13AF73G]
FX This work is supported by the Precipitation Measuring Mission under
project NNX13AF73G (Headquarter Manager: R. Kakar), NASA Earth Science
Division. The authors thank the reviewers' many constructive comments
that helped improve the manuscript.
NR 72
TC 3
Z9 3
U1 0
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 SEP 16
PY 2013
VL 118
IS 17
BP 9673
EP 9689
DI 10.1002/jgrd.50776
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 232JH
UT WOS:000325489300028
ER
PT J
AU Justice, CO
Roman, MO
Csiszar, I
Vermote, EF
Wolfe, RE
Hook, SJ
Friedl, M
Wang, ZS
Schaaf, CB
Miura, T
Tschudi, M
Riggs, G
Hall, DK
Lyapustin, AI
Devadiga, S
Davidson, C
Masuoka, EJ
AF Justice, Christopher O.
Roman, Miguel O.
Csiszar, Ivan
Vermote, Eric F.
Wolfe, Robert E.
Hook, Simon J.
Friedl, Mark
Wang, Zhuosen
Schaaf, Crystal B.
Miura, Tomoaki
Tschudi, Mark
Riggs, George
Hall, Dorothy K.
Lyapustin, Alexei I.
Devadiga, Sadashiva
Davidson, Carol
Masuoka, Edward J.
TI Land and cryosphere products from Suomi NPP VIIRS: Overview and status
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE satellite remote sensing; VIIRS; land surface; infrared; visible; global
change research
ID IMAGING SPECTRORADIOMETER MODIS; SURFACE TEMPERATURE; ALBEDO;
REFLECTANCE; VALIDATION; ALGORITHM; COVER; EMISSIVITY; MODELS; BRDF
AB The Visible Infrared Imaging Radiometer Suite (VIIRS) instrument was launched in October 2011 as part of the Suomi National Polar-Orbiting Partnership (S-NPP). The VIIRS instrument was designed to improve upon the capabilities of the operational Advanced Very High Resolution Radiometer and provide observation continuity with NASA's Earth Observing System's Moderate Resolution Imaging Spectroradiometer (MODIS). Since the VIIRS first-light images were received in November 2011, NASA- and NOAA-funded scientists have been working to evaluate the instrument performance and generate land and cryosphere products to meet the needs of the NOAA operational users and the NASA science community. NOAA's focus has been on refining a suite of operational products known as Environmental Data Records (EDRs), which were developed according to project specifications under the National Polar-Orbiting Environmental Satellite System. The NASA S-NPP Science Team has focused on evaluating the EDRs for science use, developing and testing additional products to meet science data needs, and providing MODIS data product continuity. This paper presents to-date findings of the NASA Science Team's evaluation of the VIIRS land and cryosphere EDRs, specifically Surface Reflectance, Land Surface Temperature, Surface Albedo, Vegetation Indices, Surface Type, Active Fires, Snow Cover, Ice Surface Temperature, and Sea Ice Characterization. The study concludes that, for MODIS data product continuity and earth system science, an enhanced suite of land and cryosphere products and associated data system capabilities are needed beyond the EDRs currently available from the VIIRS.
C1 [Justice, Christopher O.] Univ Maryland, Dept Geog Sci, College Pk, MD 20782 USA.
[Roman, Miguel O.; Vermote, Eric F.; Wolfe, Robert E.; Devadiga, Sadashiva; Davidson, Carol; Masuoka, Edward J.] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA.
[Csiszar, Ivan] NOAA, Ctr Satellite Applicat & Res, College Pk, MD USA.
[Hook, Simon J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Friedl, Mark] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Wang, Zhuosen; Schaaf, Crystal B.] Univ Massachusetts, Dept Environm Earth & Ocean Sci, Boston, MA 02125 USA.
[Wang, Zhuosen; Schaaf, Crystal B.] Boston Univ, Dept Earth & Environm, Ctr Remote Sensing, Boston, MA 02215 USA.
[Miura, Tomoaki] Univ Hawaii Manoa, Dept Nat Resources & Environm Management, Honolulu, HI 96822 USA.
[Tschudi, Mark] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA.
[Riggs, George] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Lanham, MD USA.
[Riggs, George; Hall, Dorothy K.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
[Lyapustin, Alexei I.] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA.
[Devadiga, Sadashiva; Davidson, Carol] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA.
RP Justice, CO (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20782 USA.
EM justice@hermes.geog.umd.edu; miguel.o.roman@nasa.gov
RI Csiszar, Ivan/D-2396-2010; Wolfe, Robert/E-1485-2012; Lyapustin,
Alexei/H-9924-2014; Miura, Tomoaki/B-5805-2008; Roman,
Miguel/D-4764-2012
OI Wolfe, Robert/0000-0002-0915-1855; Lyapustin,
Alexei/0000-0003-1105-5739; Roman, Miguel/0000-0003-3953-319X
NR 37
TC 39
Z9 39
U1 4
U2 34
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 SEP 16
PY 2013
VL 118
IS 17
BP 9753
EP 9765
DI 10.1002/jgrd.50771
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 232JH
UT WOS:000325489300033
ER
PT J
AU Bauer, SE
Ault, AP
Prather, KA
AF Bauer, Susanne E.
Ault, Andrew P.
Prather, Kimberly A.
TI Evaluation of aerosol mixing state classes in the GISS modelE-MATRIX
climate model using single-particle mass spectrometry measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE mixing state
ID GENERAL-CIRCULATION MODEL; LOS-ANGELES; SIZE DISTRIBUTIONS; PARTICULATE
MATTER; SULFATE AEROSOLS; EVENTS; CHEMISTRY; VARIABILITY; NUCLEATION;
TRANSPORT
AB Aerosol particles in the atmosphere are composed of multiple chemical species. The aerosol mixing state, which describes how chemical species are mixed at the single-particle level, provides critical information on microphysical characteristics that determine the interaction of aerosols with the climate system. The evaluation of mixing state has become the next challenge. This study uses aerosol time-of-flight mass spectrometry (ATOFMS) data and compares the results to those of the Goddard Institute for Space Studies modelE-MATRIX (Multiconfiguration Aerosol TRacker of mIXing state) model, a global climate model that includes a detailed aerosol microphysical scheme. We use data from field campaigns that examine a variety of air mass regimens (urban, rural, and maritime). At all locations, polluted areas in California (Riverside, La Jolla, and Long Beach), a remote location in the Sierra Nevada Mountains (Sugar Pine) and observations from Jeju (South Korea), the majority of aerosol species are internally mixed. Coarse aerosol particles, those above 1 mu m, are typically aged, such as coated dust or reacted sea-salt particles. Particles below 1 mu m contain large fractions of organic material, internally mixed with sulfate and black carbon, and few external mixtures. We conclude that observations taken over multiple weeks characterize typical air mass types at a given location well; however, due to the instrumentation, we could not evaluate mass budgets. These results represent the first detailed comparison of single-particle mixing states in a global climate model with real-time single-particle mass spectrometry data, an important step in improving the representation of mixing state in global climate models.
C1 [Bauer, Susanne E.] Columbia Univ, Ctr Climate Syst Res, Earth Inst, New York, NY 10025 USA.
[Ault, Andrew P.; Prather, Kimberly A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Prather, Kimberly A.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
RP Bauer, SE (reprint author), Columbia Univ, Ctr Climate Syst Res, Earth Inst, Broadway 2880, New York, NY 10025 USA.
EM Susanne.Bauer@Columbia.edu
RI Bauer, Susanne/P-3082-2014; Prather, Kimberly/A-3892-2008; Ault,
Andrew/E-4594-2011
OI Prather, Kimberly/0000-0003-3048-9890; Ault, Andrew/0000-0002-7313-8559
FU NASA MAP program Modeling, Analysis, and Prediction of Climate
Variability and Change [NN-H-04-Z-YS-008-N, NN-H-08-Z-DA-001-N];
California Air Resources Board (CARB) (Los Angeles, Riverside, and San
Diego); California Energy Commission (CEC) (Sugar Pine); Atmospheric
Brown Clouds project under the United Nations Environmental Program
(ABC) (Gosan, Korea); Department of Energy Global Change Education
Program Graduate Research Environmental Fellowship (GCEP-GREF)
FX This research was supported by the NASA MAP program Modeling, Analysis,
and Prediction of Climate Variability and Change (NN-H-04-Z-YS-008-N and
NN-H-08-Z-DA-001-N). 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. Funding for
the field studies discussed came from the California Air Resources Board
(CARB) (Los Angeles, Riverside, and San Diego), California Energy
Commission (CEC) (Sugar Pine), and Atmospheric Brown Clouds project
under the United Nations Environmental Program (ABC) (Gosan, Korea). A.
A. is grateful for a Department of Energy Global Change Education
Program Graduate Research Environmental Fellowship (GCEP-GREF). Jessie
Creamean, Cassandra Gaston, Xueying Qin, Steve Toner, Ying Wang, and
Aihua Zhu are thankfully acknowledged for their contributions during
data collection. V. Ramanathan and S. Yoon are thanked for their role in
the Gosan measurements.
NR 45
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U2 44
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 SEP 16
PY 2013
VL 118
IS 17
BP 9834
EP 9844
DI 10.1002/jgrd.50700
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 232JH
UT WOS:000325489300039
ER
PT J
AU Lewis, JR
Welton, EJ
Molod, AM
Joseph, E
AF Lewis, Jasper R.
Welton, Ellsworth J.
Molod, Andrea M.
Joseph, Everette
TI Improved boundary layer depth retrievals from MPLNET
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE PBL depth; MPLNET; mixing layer; lidar
ID LIDAR BACKSCATTER PROFILES; ENTRAINMENT ZONE THICKNESS; RADIO
OCCULTATION DATA; MIXING HEIGHT; TOP; RADIATION; NETWORK; CLOUDS; WIND
AB Continuous lidar observations of the planetary boundary layer (PBL) depth have been made at the Micropulse Lidar Network (MPLNET) site in Greenbelt, Maryland, since April 2001. However, because of issues with the operational PBL depth algorithm, the data are not reliable for determining seasonal and diurnal trends. Therefore, an improved PBL depth algorithm has been developed which uses a combination of the wavelet technique and image processing. The new algorithm is less susceptible to contamination by clouds and residual layers and, in general, produces lower PBL depths. A 2010 comparison shows the operational algorithm overestimates the daily mean PBL depth when compared to the improved algorithm (1.85 and 1.07 km, respectively). The improved MPLNET PBL depths are validated using radiosonde comparisons, which suggests the algorithm performs well to determine the depth of a fully developed PBL. A comparison with the Goddard Earth Observing System version 5 (GEOS-5) model suggests that the model may underestimate the maximum daytime PBL depth by approximate to 410 m during the spring and summer. The best agreement between MPLNET and GEOS-5 occurred during the fall and they differed the most in the winter.
C1 [Lewis, Jasper R.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Lewis, Jasper R.; Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Molod, Andrea M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Molod, Andrea M.] Global Modeling & Assimilat Off, Greenbelt, MD USA.
[Joseph, Everette] Howard Univ, Beltsville Ctr Climate Syst Observat, Washington, DC 20059 USA.
RP Lewis, JR (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM jasper.r.lewis@nasa.gov
FU NASA
FX The authors would like to acknowledge the support of Larry Belcher for
processing the lidar data, Lawrence Takacs who ran the model
simulations, and the MPLNET staff for their efforts in establishing and
maintaining the GSFC site. 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 NASA Micropulse Lidar Network is funded by the NASA Earth
Observing System and Radiation Sciences Program.
NR 44
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U1 1
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 SEP 16
PY 2013
VL 118
IS 17
BP 9870
EP 9879
DI 10.1002/jgrd.50570
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 232JH
UT WOS:000325489300041
ER
PT J
AU Ham, SH
Sohn, BJ
Kato, S
Satoh, M
AF Ham, Seung-Hee
Sohn, Byung-Ju
Kato, Seiji
Satoh, Masaki
TI Vertical structure of ice cloud layers from CloudSat and CALIPSO
measurements and comparison to NICAM simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE ice cloud; vertical structure; CloudSat; CALIPSO; NICAM
ID RESOLVING MODEL; CIRRUS CLOUDS; MICROPHYSICAL PROPERTIES; PART II;
ALGORITHM; EVOLUTION; RETRIEVAL; PROFILES; WAVE; PARAMETERIZATION
AB The shape of the vertical profile of ice cloud layers is examined using 4months of CloudSat and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) global measurements taken on January, April, July, and October 2007. Ice clouds are selected using temperature profiles when the cloud base is located above the 253K temperature level. The obtained ice water content (IWC), effective radius, or extinction coefficient profiles are normalized by their layer mean values and are expressed in the normalized vertical coordinate, which is defined as 0 and 1 at the cloud base and top heights, respectively. Both CloudSat and CALIPSO observations show that the maximum in the IWC and extinction profiles shifts toward the cloud bottom, as the cloud depth increases. In addition, clouds with a base reaching the surface in a high-latitude region show that the maximum peak of the IWC and extinction profiles occurs near the surface, which is presumably due to snow precipitation. CloudSat measurements show that the seasonal difference in normalized cloud vertical profiles is not significant, whereas the normalized cloud vertical profile significantly varies depending on the cloud type and the presence of precipitation. It is further examined if the 7day Nonhydrostatic Icosahedral Atmospheric Model (NICAM) simulation results from 25 December 2006 to 1 January 2007 generate similar cloud profile shapes. NICAM IWC profiles also show maximum peaks near the cloud bottom for thick cloud layers and maximum peaks at the cloud bottom for low-level clouds near the surface. It is inferred that oversized snow particles in the NICAM cloud scheme produce a more vertically inhomogeneous IWC profile than observations due to quick sedimentation.
C1 [Ham, Seung-Hee; Kato, Seiji] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Sohn, Byung-Ju] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea.
[Satoh, Masaki] Univ Tokyo, Atmosphere & Ocean Res Inst, Chiba, Japan.
RP Ham, SH (reprint author), NASA, Langley Res Ctr, 100 NASA Rd,Mailstop 420, Hampton, VA 23681 USA.
EM seung-hee.ham@nasa.gov
RI Satoh, Masaki/G-3325-2015
OI Satoh, Masaki/0000-0003-3580-8897
FU Korea Meteorological Administration Research and Development Program
[CATER 2012-2061]; CERES; NASA Energy Water Cycle Study (NEWS) project;
NASA Postdoctoral Program at the NASA Langley Research Center
FX This work was funded by the Korea Meteorological Administration Research
and Development Program under grant CATER 2012-2061. The first and third
authors (S.-H. Ham and S. Kato) were also supported by CERES and the
NASA Energy Water Cycle Study (NEWS) project. The first author was also
supported by the NASA Postdoctoral Program at the NASA Langley Research
Center, administered by Oak Ridge Associated Universities (ORAU). We
also thank Patrick Taylor in LASA Langley Research Center for
proofreading the manuscript.
NR 47
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Z9 3
U1 4
U2 16
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 SEP 16
PY 2013
VL 118
IS 17
BP 9930
EP 9947
DI 10.1002/jgrd.50582
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 232JH
UT WOS:000325489300046
ER
PT J
AU Lee, J
Hsu, NC
Bettenhausen, C
Sayer, AM
AF Lee, Jaehwa
Hsu, N. Christina
Bettenhausen, Corey
Sayer, Andrew M.
TI Retrieval of aerosol optical depth under thin cirrus from MODIS:
Application to an ocean algorithm
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosol; AOD; cirrus; correction; MODIS
ID RADIATIVE-TRANSFER CODE; GROUND-BASED LIDAR; SATELLITE DATA; ATMOSPHERIC
CORRECTION; VECTOR VERSION; CLOUDS; VALIDATION; AERONET; REFLECTANCE;
CHANNELS
AB A strategy for retrieving aerosol optical depth (AOD) under conditions of thin cirrus coverage from the Moderate Resolution Imaging Spectroradiometer (MODIS) is presented. We adopt an empirical method that derives the cirrus contribution to measured reflectance in seven bands from the visible to shortwave infrared (0.47, 0.55, 0.65, 0.86, 1.24, 1.63, and 2.12 mu m, commonly used for AOD retrievals) by using the correlations between the top-of-atmosphere (TOA) reflectance at 1.38 mu m and these bands. The 1.38 mu m band is used due to its strong absorption by water vapor and allows us to extract the contribution of cirrus clouds to TOA reflectance and create cirrus-corrected TOA reflectances in the seven bands of interest. These cirrus-corrected TOA reflectances are then used in the aerosol retrieval algorithm to determine cirrus-corrected AOD. The cirrus correction algorithm reduces the cirrus contamination in the AOD data as shown by a decrease in both magnitude and spatial variability of AOD over areas contaminated by thin cirrus. Comparisons of retrieved AOD against Aerosol Robotic Network observations at Nauru in the equatorial Pacific reveal that the cirrus correction procedure improves the data quality: the percentage of data within the expected error +/-(0.03+0.05xAOD) increases from 40% to 80% for cirrus-corrected points only and from 80% to 86% for all points (i.e., both corrected and uncorrected retrievals). Statistical comparisons with Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) retrievals are also carried out. A high correlation (R=0.89) between the CALIOP cirrus optical depth and AOD correction magnitude suggests potential applicability of the cirrus correction procedure to other MODIS-like sensors.
C1 [Lee, Jaehwa] Univ Maryland, Earth Syst Sci Inter disciplinary Ctr, College Pk, MD 20742 USA.
[Lee, Jaehwa; Hsu, N. Christina; Bettenhausen, Corey; Sayer, Andrew M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bettenhausen, Corey] Sci Syst & Applicat Inc, Lanham, MD USA.
[Sayer, Andrew M.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
RP Lee, J (reprint author), Univ Maryland, Earth Syst Sci Inter disciplinary Ctr, College Pk, MD 20742 USA.
EM jaehwa.lee@nasa.gov
RI Sayer, Andrew/H-2314-2012
OI Sayer, Andrew/0000-0001-9149-1789
FU NASA's EOS program
FX This project was funded by the NASA's EOS program, managed by Hal
Maring. The MODIS data were obtained from the Level 1 and Atmosphere
Archive and Distribution System (LAADS), and the CALIOP data were
obtained from the NASA Langley Research Center Atmospheric Science Data
Center. We thank the AERONET staff, PIs, and site managers for their
effort in establishing and maintaining Nauru site (B. N. Holben, R.
Wagener, L. Jones, and K. Nitschke). The authors are grateful to the
anonymous reviewers for their constructive comments and suggestions.
NR 43
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U1 0
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 SEP 16
PY 2013
VL 118
IS 17
BP 10111
EP 10124
DI 10.1002/jgrd.50806
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 232JH
UT WOS:000325489300010
ER
PT J
AU Chatterjee, A
Engelen, RJ
Kawa, SR
Sweeney, C
Michalak, AM
AF Chatterjee, Abhishek
Engelen, Richard J.
Kawa, Stephan R.
Sweeney, Colm
Michalak, Anna M.
TI Background error covariance estimation for atmospheric CO2 data
assimilation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE background error covariance matrix; variational data assimilation;
atmospheric CO2; spatial and temporal CO2 variations; GOSAT CO2; NMC
method
ID INFRARED SATELLITE RADIANCES; RETRIEVAL ALGORITHM; CARBON-DIOXIDE;
SYSTEM; STATISTICS; TRANSPORT; MODEL; STRATOSPHERE; SINKS; SPECTROMETER
AB In any data assimilation framework, the background error covariance statistics play the critical role of filtering the observed information and determining the quality of the analysis. For atmospheric CO2 data assimilation, however, the background errors cannot be prescribed via traditional forecast or ensemble-based techniques as these fail to account for the uncertainties in the carbon emissions and uptake, or for the errors associated with the CO2 transport model. We propose an approach where the differences between two modeled CO2 concentration fields, based on different but plausible CO2 flux distributions and atmospheric transport models, are used as a proxy for the statistics of the background errors. The resulting error statistics: (1) vary regionally and seasonally to better capture the uncertainty in the background CO2 field, and (2) have a positive impact on the analysis estimates by allowing observations to adjust predictions over large areas. A state-of-the-art four-dimensional variational (4D-VAR) system developed at the European Centre for Medium-Range Weather Forecasts (ECMWF) is used to illustrate the impact of the proposed approach for characterizing background error statistics on atmospheric CO2 concentration estimates. Observations from the Greenhouse gases Observing SATellite IBUKI (GOSAT) are assimilated into the ECMWF 4D-VAR system along with meteorological variables, using both the new error statistics and those based on a traditional forecast-based technique. Evaluation of the four-dimensional CO2 fields against independent CO2 observations confirms that the performance of the data assimilation system improves substantially in the summer, when significant variability and uncertainty in the fluxes are present.
C1 [Chatterjee, Abhishek] Univ Michigan, Dept Civil & Environm Engn, Ann Arbor, MI 48109 USA.
[Chatterjee, Abhishek; Michalak, Anna M.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA.
[Engelen, Richard J.] European Ctr Medium Range Weather Forecasts, Reading, Berks, England.
[Kawa, Stephan R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sweeney, Colm] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Sweeney, Colm] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO USA.
RP Chatterjee, A (reprint author), NCAR Boulder, Data Assimilat Res Sect, Boulder, CO USA.
EM abhishek@ucar.edu
RI Chatterjee, Abhishek/E-6296-2017
OI Chatterjee, Abhishek/0000-0002-3680-0160
FU National Aeronautics and Space Administration (NASA) [NNX09AO10H,
NNX12AB90G]; European Commission through the MACC [218793]
FX The authors thank Derek Posselt, Peter Adriaens and three anonymous
reviewers for fruitful comments and discussions regarding this work, the
many people at ECMWF who helped build the tracer data assimilation
system, and partners within the GEMS and MACC projects. This work was
supported by the National Aeronautics and Space Administration (NASA)
through Earth System Science Fellowship for Abhishek Chatterjee, under
grant NNX09AO10H. Additional support was provided through NASA grant
NNX12AB90G. The work of Richard Engelen was funded through the MACC
project, which is funded by the European Commission under the Seventh
Research Framework Programme, contract 218793. The work of Stephan Kawa
was supported through the NASA Carbon Cycle Science and Atmospheric
CO2 Observations from Space opportunities. TCCON data were
obtained from the TCCON Data Archive, operated by the California
Institute of Technology from the website at
http://tccon.ipac.caltech.edu/. Finally, the GOSAT-ACOS data were
produced by the ACOS/OCO-2 project at the Jet Propulsion Laboratory,
California Institute of Technology, and obtained from the ACOS/OCO-2
data archive maintained at the NASA Goddard Earth Science Data and
Information Services Center.
NR 68
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U1 0
U2 13
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 SEP 16
PY 2013
VL 118
IS 17
BP 10140
EP 10154
DI 10.1002/jgrd.50654
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 232JH
UT WOS:000325489300005
ER
PT J
AU Muller, IA
Brunner, B
Coleman, M
AF Mueller, Inigo A.
Brunner, Benjamin
Coleman, Max
TI Isotopic evidence of the pivotal role of sulfite oxidation in shaping
the oxygen isotope signature of sulfate
SO CHEMICAL GEOLOGY
LA English
DT Article
DE Oxygen isotopes; Sulfate; Abiotic sulfite oxidation; Oxygen exchange
ID ACID-MINE DRAINAGE; COASTAL MARINE SEDIMENT; BISULFITE ION; FERROUS
IRON; THIOBACILLUS-FERROOXIDANS; ELEMENTAL SULFUR; BACTERIAL OXIDATION;
DISSOLVED-OXYGEN; PYRITE OXIDATION; PHASE OXIDATION
AB The oxygen isotope composition of sulfate serves as an archive of oxidative sulfur cycling. Studies on the aerobic oxidation of reduced sulfur compounds showed discrepancies in the relative incorporation of oxygen from dissolved molecular oxygen (O2) and water (H2O) into newly formed sulfate, which likely result from slight differences in the production and consumption rate of sulfoxy intermediates that exchange oxygen isotopes with water. Sulfite is often considered the final sulfoxy intermediate in the oxidation of reduced sulfur compounds to sulfate and its residence time strongly affects the oxygen isotope signature of produced sulfate. However, data on the oxygen isotope signature of sulfate derived from sulfite oxidation are scarce.
We determined the oxygen isotope effects of abiotic oxidation of sulfite with O-2 or ferric iron (Fe3+) under different pH conditions (pH 1, 4.9 and 13.3). These parameters impact the relative contribution of oxygen from H2O and O-2 to the produced sulfate, and control the competition between the rates of oxygen isotope exchange between sulfite and water and the sulfite oxidation. There is a striking overlap in the range of oxygen isotope offsets between sulfate and water from our experiments at different chemical conditions (Delta O-18(SO4 - H2O) from 5.9% for anaerobic oxidation with Fe3+ up to 17.6% for oxidation at low pH with O-2 as sole oxidant, respectively) with the variations in the oxygen isotope composition of sulfate derived from oxidative processes in the environment. This implies that oxygen isotope effects during sulfite oxidation largely control the isotope signature of sulfate derived from the oxidation of sulfur compounds. However, our results also show that preexisting non-equilibrium isotope signatures of sulfite are likely partially preserved in the final sulfate product under most environmental conditions. Our study furthermore provides a mechanistic explanation for positive isotope offsets between the oxygen isotope composition of sulfate and water observed in anoxic pyrite oxidation experiments with Fe3+ as the sole oxidizing agent. This apparently inverse isotope effect is caused by the interplay between sulfite-water oxygen exchange and normal kinetic isotope fractionation effects during sulfite oxidation, the former driving the isotope composition towards the isotope equilibrium fractionation between sulfite and water, inducing a positive offset whereas the latter induces a negative offset. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Mueller, Inigo A.; Brunner, Benjamin] Max Planck Inst Marine Microbiol, Biogeochem Dept, D-28359 Bremen, Germany.
[Mueller, Inigo A.] Univ Bremen, Ctr Marine Environm Sci, MARUM, D-28359 Bremen, Germany.
[Brunner, Benjamin] Aarhus Univ, Dept Biosci, Ctr Geomicrobiol, DK-8000 Aarhus C, Denmark.
[Coleman, Max] CALTECH, NASA, Jet Prop Lab, Planetary Surface Instruments Grp, Pasadena, CA 91109 USA.
RP Muller, IA (reprint author), Max Planck Inst Marine Microbiol, Biogeochem Dept, Celsiusstr 1, D-28359 Bremen, Germany.
EM imueller@mpi-bremen.de
FU NASA Astrobiology Institute (NAI-WARC); National Aeronautics and Space
Administration (NASA); MARUM
FX We would like to acknowledge T. Max for the help with the mass
spectrometer, P. Stief for the introduction to the application of oxygen
microsensors and A.V. Turchyn and N. Balci for inspiring discussions.
The authors thank S.M. Bernasconi for isotope analysis, W. Bach and T.G.
Ferdelman for their support and the Max Planck Society as well as the
MARUM for funding of this work. We would like to acknowledge the
anonymous reviewers and the Editor D. Hilton for their comments that
helped focusing and improving our manuscript. The contribution of M.C.
was carried out at the NASA Jet Propulsion Laboratory (JPL), California
Institute of Technology, under contract with the National Aeronautics
and Space Administration (NASA), with support from the NASA Astrobiology
Institute (NAI-WARC).
NR 72
TC 5
Z9 5
U1 3
U2 38
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2541
EI 1878-5999
J9 CHEM GEOL
JI Chem. Geol.
PD SEP 16
PY 2013
VL 354
BP 186
EP 202
DI 10.1016/j.chemgeo.2013.05.009
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 235WE
UT WOS:000325751200015
ER
PT J
AU Claudepierre, SG
Mann, IR
Takahashi, K
Fennell, JF
Hudson, MK
Blake, JB
Roeder, JL
Clemmons, JH
Spence, HE
Reeves, GD
Baker, DN
Funsten, HO
Friedel, RHW
Henderson, MG
Kletzing, CA
Kurth, WS
MacDowall, RJ
Smith, CW
Wygant, JR
AF Claudepierre, S. G.
Mann, I. R.
Takahashi, K.
Fennell, J. F.
Hudson, M. K.
Blake, J. B.
Roeder, J. L.
Clemmons, J. H.
Spence, H. E.
Reeves, G. D.
Baker, D. N.
Funsten, H. O.
Friedel, R. H. W.
Henderson, M. G.
Kletzing, C. A.
Kurth, W. S.
MacDowall, R. J.
Smith, C. W.
Wygant, J. R.
TI Van Allen Probes observation of localized drift resonance between
poloidal mode ultra-low frequency waves and 60 keV electrons
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE drift-resonance; ultra-low frequency; radiation belt electron; radial
diffusion; inner magnetosphere
ID RADIATION BELT; ACCELERATION; PARTICLES
AB We present NASA Van Allen Probes observations of wave-particle interactions between magnetospheric ultra-low frequency (ULF) waves and energetic electrons (20-500 keV) on 31 October 2012. The ULF waves are identified as the fundamental poloidal mode oscillation and are excited following an interplanetary shock impact on the magnetosphere. Large amplitude modulations in energetic electron flux are observed at the same period (approximate to 3 min) as the ULF waves and are consistent with a drift-resonant interaction. The azimuthal mode number of the interacting wave is estimated from the electron measurements to be similar to 40, based on an assumed symmetric drift resonance. The drift-resonant interaction is observed to be localized and occur over 5-6 wave cycles, demonstrating peak electron flux modulations at energies similar to 60 keV. Our observation clearly shows electron drift resonance with the fundamental poloidal mode, the energy dependence of the amplitude and phase of the electron flux modulations providing strong evidence for such an interaction. Significantly, the observation highlights the importance of localized wave-particle interactions for understanding energetic particle dynamics in the inner magnetosphere, through the intermediary of ULF waves.
C1 [Claudepierre, S. G.; Fennell, J. F.; Blake, J. B.; Roeder, J. L.; Clemmons, J. H.] Aerosp Corp, Dept Space Sci, El Segundo, CA 90245 USA.
[Mann, I. R.] Univ Alberta, Dept Phys, Edmonton, AB, Canada.
[Takahashi, K.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Hudson, M. K.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Reeves, G. D.; Funsten, H. O.; Friedel, R. H. W.; Henderson, M. G.] Los Alamos Natl Lab, Space & Atmospher Sci Grp, Los Alamos, NM USA.
[Baker, D. N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Kletzing, C. A.; Kurth, W. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[MacDowall, R. J.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Smith, C. W.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Smith, C. W.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Wygant, J. R.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
RP Claudepierre, SG (reprint author), Aerosp Corp, Dept Space Sci, El Segundo, CA 90245 USA.
EM seth@aero.org
RI Friedel, Reiner/D-1410-2012; Funsten, Herbert/A-5702-2015; Reeves,
Geoffrey/E-8101-2011; Henderson, Michael/A-3948-2011; Claudepierre,
Seth/A-6109-2012;
OI Friedel, Reiner/0000-0002-5228-0281; Funsten,
Herbert/0000-0002-6817-1039; Reeves, Geoffrey/0000-0002-7985-8098;
Henderson, Michael/0000-0003-4975-9029; Spence,
Harlan/0000-0002-2526-2205; Kletzing, Craig/0000-0002-4136-3348; Kurth,
William/0000-0002-5471-6202; Clemmons, James/0000-0002-5298-5222
FU JHU/APL [967399, 921647]; NASA' [NAS5-01072]; NASA [NNX10AK93G];
Canadian Space Agency; Monitoring, Analyzing and Assessing Radiation
Belt Loss and Energization (MAARBLE) consortium; European Community
[284520]; Canadian NSERC
FX This work was supported by RBSP-ECT funding provided by JHU/APL contract
967399 and EMFISIS funding provided by JHU/APL contract 921647, both
under NASA's prime contract NAS5-01072. Work at JHU/APL was supported by
NASA grant NNX10AK93G. The OMNI data were obtained from the GSFC/SPDF
OMNIWeb interface at http://omniweb.gsfc.nasa.gov. CARISMA is operated
by the University of Alberta, funded by the Canadian Space Agency. This
work is supported in part by participation in the Monitoring, Analyzing
and Assessing Radiation Belt Loss and Energization (MAARBLE) consortium.
MAARBLE has received funding from the European Community's Seventh
Framework Programme (FP7-SPACE-2010-1, SP1 Cooperation, Collaborative
project) under grant agreement 284520. This paper reflects only the
authors' views and the Union is not liable for any use that may be made
of the information contained herein. I.R.M. is supported by a Discovery
grant from Canadian NSERC. One author (S.G.C.) would like to thank
Jeremy Faden and all of the developers of Autoplot, and Paul O'Brien for
making available useful analysis routines.
NR 13
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U1 1
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 SEP 16
PY 2013
VL 40
IS 17
BP 4491
EP 4497
DI 10.1002/grl.50901
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 232JP
UT WOS:000325490300004
ER
PT J
AU Xu, Y
Rignot, E
Fenty, I
Menemenlis, D
Flexas, MM
AF Xu, Yun
Rignot, Eric
Fenty, Ian
Menemenlis, Dimitris
Flexas, M. Mar
TI Subaqueous melting of Store Glacier, west Greenland from
three-dimensional, high-resolution numerical modeling and ocean
observations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Greenland; glaciology; ocean modeling; climate change; hydrology
ID ICE-SHEET; TIDEWATER GLACIERS; EAST GREENLAND; WATERS; FJORD;
PARAMETERIZATION; ACCELERATION
AB We present three-dimensional, high-resolution simulations of ice melting at the calving face of Store Glacier, a tidewater glacier in West Greenland, using the Massachusetts Institute of Technology general circulation model. We compare the simulated ice melt with an estimate derived from oceanographic data. The simulations show turbulent upwelling and spreading of the freshwater-laden plume along the ice face and the vigorous melting of ice at rates of meters per day. The simulated August 2010 melt rate of 2.00.3m/d is within uncertainties of the melt rate of 3.01.0m/d calculated from oceanographic data. Melting is greatest at depth, above the subglacial channels, causing glacier undercutting. Melt rates increase proportionally to thermal forcing raised to the power of 1.2-1.6 and to subglacial water flux raised to the power of 0.5-0.9. Therefore, in a warmer climate, Store Glacier melting by ocean may increase from both increased ocean temperature and subglacial discharge.
C1 [Xu, Yun; Rignot, Eric] Univ Calif Irvine, Irvine, CA 92697 USA.
[Rignot, Eric; Fenty, Ian; Menemenlis, Dimitris; Flexas, M. Mar] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Xu, Y (reprint author), Univ Calif Irvine, 240G Rowland Hall, Irvine, CA 92697 USA.
EM yunx@uci.edu
RI Rignot, Eric/A-4560-2014
OI Rignot, Eric/0000-0002-3366-0481
FU National Aeronautics and Space Administration
FX We thank Roman Motyka and an anonymous reviewer for their constructive
comments. We thank Jan H. van Angelen and Michiel R. van den Broeke
(Utrecht University) for providing the daily RACMO runoff data. This
work was performed at the University of California Irvine under a
contract with the National Aeronautics and Space Administration
Cryosphere Science Programs.
NR 20
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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 SEP 16
PY 2013
VL 40
IS 17
BP 4648
EP 4653
DI 10.1002/grl.50825
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 232JP
UT WOS:000325490300034
ER
PT J
AU Gorkavyi, N
Rault, DF
Newman, PA
da Silva, AM
Dudorov, AE
AF Gorkavyi, Nick
Rault, D. F.
Newman, P. A.
da Silva, A. M.
Dudorov, A. E.
TI New stratospheric dust belt due to the Chelyabinsk bolide
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE NPP; Suomi; aerosol; bolide; Chelyabinsk; stratosphere
ID PLUME
AB The Ozone Mapping Profiler Suite (OMPS) Limb Profiler (LP) on the recently launched NASA/NOAA NPP/Suomi satellite detected aerosol excess in the mid-stratosphere (25-45 km altitude) between 50 degrees N and 70 degrees N latitudes. OMPS/LP observations trace this aerosol plume to the meteor that struck near Chelyabinsk, Russia on 15 February 2013. This new dust layer, located above the Junge aerosol layer, has persisted over at least a 3 month period. Material collected on the ground following the bolide explosion showed that the meteor was mostly composed of olivine and pyroxenes. Simulations using Lagrangian and Eulerian atmospheric models trace the plume back to Chelyabinsk and confirm that the plume altitude was at altitudes between 25 and 45 km. The models also confirm the plume circumpolar longitudinal spreading observed by OMPS/LP, with propagation speeds up to 85 m/s.
C1 [Gorkavyi, Nick] Sci Syst & Applicat Inc, Lanham, MD 20760 USA.
[Rault, D. F.] Morgan State Univ, Columbia, MD USA.
[Newman, P. A.; da Silva, A. M.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Dudorov, A. E.] Chelyabinsk State Univ, Chelyabinsk, Russia.
RP Gorkavyi, N (reprint author), Sci Syst & Applicat Inc, Suite 600,10210 Greenbelt Rd, Lanham, MD 20760 USA.
EM nick.gorkavyi@nasa.gov
RI Newman, Paul/D-6208-2012; Dudorov, Alexander/P-4773-2015
OI Newman, Paul/0000-0003-1139-2508;
NR 18
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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 SEP 16
PY 2013
VL 40
IS 17
BP 4728
EP 4733
DI 10.1002/grl.50788
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 232JP
UT WOS:000325490300048
ER
PT J
AU McGillen, MR
Fleming, EL
Jackman, CH
Burkholder, JB
AF McGillen, Max R.
Fleming, Eric L.
Jackman, Charles H.
Burkholder, James B.
TI CFCl3 (CFC-11): UV absorption spectrum temperature dependence
measurements and the impact on its atmospheric lifetime and uncertainty
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ozone depleting substance; photolysis; chlorofluorocarbon; UV cross
section
ID ULTRAVIOLET-ABSORPTION; CROSS-SECTIONS; CHLOROMETHANES; METHANES
AB CFCl3 (CFC-11) is both an atmospheric ozone-depleting and potent greenhouse gas that is removed primarily via stratospheric UV photolysis. Uncertainty in the temperature dependence of its UV absorption spectrum is a significant contributing factor to the overall uncertainty in its global lifetime and, thus, model calculations of stratospheric ozone recovery and climate change. In this work, the CFC-11 UV absorption spectrum was measured over a range of wavelength (184.95-230nm) and temperature (216-296K). We report a spectrum temperature dependence that is less than that currently recommended for use in atmospheric models. The impact on its atmospheric lifetime was quantified using a 2-D model and the spectrum parameterization developed in this work. The calculated global annually averaged lifetime was 58.1 +/- 0.7 years (2 sigma uncertainty due solely to the spectrum uncertainty). The lifetime is slightly reduced and the uncertainty significantly reduced from that obtained using current UV spectrum recommendations.
C1 [McGillen, Max R.; Burkholder, James B.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA.
[McGillen, Max R.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Fleming, Eric L.; Jackman, Charles H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fleming, Eric L.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Burkholder, JB (reprint author), NOAA, 325 Broadway, Boulder, CO 80305 USA.
EM James.B.Burkholder@noaa.gov
RI McGillen, Max/G-5196-2011; Jackman, Charles/D-4699-2012; Burkholder,
James/H-4914-2013; Manager, CSD Publications/B-2789-2015
OI McGillen, Max/0000-0002-1623-5985;
FU NOAAs Climate Goal; NASAs Atmospheric Composition Program Laboratory
FX This work was supported in part by NOAAs Climate Goal and NASAs
Atmospheric Composition Program Laboratory Studies and Modeling and
Analysis Programs.
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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 SEP 16
PY 2013
VL 40
IS 17
BP 4772
EP 4776
DI 10.1002/grl.50915
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 232JP
UT WOS:000325490300056
ER
PT J
AU Quick, LC
Barnouin, OS
Prockter, LM
Patterson, GW
AF Quick, Lynnae C.
Barnouin, Olivier S.
Prockter, Louise M.
Patterson, G. Wesley
TI Constraints on the detection of cryovolcanic plumes on Europa
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Europa; Cryovolcanism; Volcanism; Geological processes; Instrumentation
ID GALILEAN SATELLITES; E-RING; ENCELADUS PLUME; WATER; ORIGIN; IO;
PARTICLES; EVOLUTION; DISCOVERY; VOLCANISM
AB Surface venting is a common occurrence on several outer solar system satellites. Spacecraft have observed plumes erupting from the geologically young surfaces of Io, Triton and Enceladus. Europa also has a relatively young surface and previous studies have suggested that cryovolcanic eruptions may be responsible for the production of low-albedo deposits surrounding lenticulae and along triple band margins and lineae. Here, we have used the projected thicknesses of these deposits as constraints to determine the lifetimes of detectable cryovolcanic plumes that may have emplaced them. In an effort to explore the feasibility of detection of the particle component of plumes by spacecraft cameras operating at visible wavelengths, we present a conservative model to estimate plume characteristics such as height, eruption velocity, and optical depth under a variety of conditions. We find that cryovolcanic plumes on Europa are likely to be fairly small in stature with heights between 2.5 and 26 km, and eruption velocities between 81 and 261 m/s, respectively. Under these conditions and assuming that plumes are products of steady eruptions with particle radii of 0.5 mu m, our model suggests that easily detectable plumes will have optical depths, tau, greater than or equal to 0.04, and that their lifetimes may be no more than 300,000 years. Plume detection may be possible if high phase angle limb observations and/or stereo imaging of the surface are undertaken in areas where eruptive activity is likely to occur. Cameras with imaging resolutions greater than 50 m/pixel should be used to make all observations. Future missions could employ the results of our model in searches for plume activity at Europa. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Quick, Lynnae C.; Barnouin, Olivier S.] Johns Hopkins Univ, Earth & Planetary Sci Dept, Baltimore, MD 21218 USA.
[Quick, Lynnae C.; Barnouin, Olivier S.; Prockter, Louise M.; Patterson, G. Wesley] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Quick, LC (reprint author), NASA, Goddard Space Flight Ctr, Code Planetary Geodynam Lab 698, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM lynnae.c.quick@nasa.gov; olivier.barnouin@jhuapl.edu;
louise.prockter@jhuapl.edu; wes.patterson@jhuapl.edu
RI Patterson, Gerald/E-7699-2015; Barnouin, Olivier/I-7475-2015
OI Barnouin, Olivier/0000-0002-3578-7750
FU NASA; Johns Hopkins University Applied Physics Laboratory Fellows and
Professors Program; Johns Hopkins University Applied Physics Laboratory
Graduate Student Fellowship
FX We gratefully acknowledge funding from the NASA Outer Planets Research
Program, the Johns Hopkins University Applied Physics Laboratory Fellows
and Professors Program, and the Johns Hopkins University Applied Physics
Laboratory Graduate Student Fellowship. We also thank Dr. Juergen
Schmidt and Dr. John Spencer for helpful suggestions that significantly
improved this manuscript.
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP 15
PY 2013
VL 86
BP 1
EP 9
DI 10.1016/j.pss.2013.06.028
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 251EO
UT WOS:000326910800001
ER
PT J
AU Waite, JH
Bell, J
Lorenz, R
Achterberge, R
Flasar, FM
AF Waite, J. H.
Bell, J.
Lorenz, R.
Achterberge, R.
Flasar, F. M.
TI A model of variability in Titan's atmospheric structure
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Titan; Cassini; Empirical model; Atmosphere; Entry; Descent; Landing
ID OCCULTATIONS; REANALYSIS; SURFACE; TEMPERATURES; DISR
AB Titan's atmosphere has been extensively studied during the Cassini-Huygens Mission. The polar environment undergoes considerable seasonal variation and is distinct from the more quiescent equatorial environment experienced by the Huygens probe in 2005. The thermal structure of the upper atmosphere is affected by interaction of Titan's atmosphere with the plasma and energetic particles in Saturn's magnetosphere or in the solar wind. Titan's polar regions, and its hydrocarbon lakes in particular, are of interest for future exploration as is the complex organic chemistry that takes place in the upper atmosphere. Thus, specific environmental models are required for future exploration. Furthermore, the models developed to support the design of Huygens had to accommodate wide uncertainties, requiring large design margins. The extensive observations by the Cassini spacecraft (and indeed Huygens itself) provide a basis for narrowing these uncertainties, notably in composition. We provide a description of these new data sets, their scientific basis, and present limitations. The empirically constrained neutral temperatures and densities presented here also have important implications for fundamental chemical modeling. The empirical modeling presented here provides constraints on these models, which will lead to improved estimations of chemical products. Therefore, the paper describes a new model of Titan's atmospheric structure to guide both scientific studies and future engineering studies of exploration of the Saturn system. Of particular interest are aero-capture and aero-braking missions that may enable future exploration of the Saturnian satellite system. (C) 2013 Published by Elsevier Ltd.
C1 [Waite, J. H.; Bell, J.] Southwest Res Inst SwRI, San Antonio, TX 78228 USA.
[Lorenz, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Flasar, F. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bell, J.] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Achterberge, R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Bell, J (reprint author), SW Res Inst, Space Sci & Engn Dept, 6220 Culebra Rd, San Antonio, TX 78228 USA.
EM jared.bell@niatnet.org
RI Flasar, F Michael/C-8509-2012; Lorenz, Ralph/B-8759-2016
OI Lorenz, Ralph/0000-0001-8528-4644
FU Cassini INMS grant through JPL; APL Janney Publication Program
FX This work was supported by the Cassini INMS grant through JPL. R.L.
would like to acknowledge the support of the APL Janney Publication
Program.
NR 40
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP 15
PY 2013
VL 86
BP 45
EP 56
DI 10.1016/j.pss.2013.05.018
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 251EO
UT WOS:000326910800004
ER
PT J
AU Bishop, JL
Loizeau, D
McKeown, NK
Saper, L
Dyar, MD
Des Marais, DJ
Parente, M
Murchie, SL
AF Bishop, Janice L.
Loizeau, Damien
McKeown, Nancy K.
Saper, Lee
Dyar, M. Darby
Des Marais, David J.
Parente, Mario
Murchie, Scott L.
TI What the ancient phyllosilicates at Mawrth Vallis can tell us about
possible habitability on early Mars
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Phyllosilicates; Reflectance spectroscopy; Water; Habitability
ID DEEP-SEA SEDIMENTS; MONTMORILLONITE-CATALYZED FORMATION; SIMULATED
MARTIAN ENVIRONMENT; GREEN COLOR TRANSITION; WIGHT HAMPSHIRE BASIN;
TO-ILLITE REACTION; CLAY-MINERALS; MICROBIAL REDUCTION; DIOCTAHEDRAL
SMECTITES; INFRARED-SPECTROSCOPY
AB Phyllosilicate deposits on Mars provide an opportunity to evaluate aqueous activity and the possibility that habitable environments may have existed during the Noachian period there. Analysis of hyperspectral visible/near-infrared (VNIR) Mars Reconnaissance Orbiter (MRO) Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) images has shown thick, complex profiles of phyllosilicates at Mawrth Vallis, Mars that are consistent with long-term aqueous activity and active chemistry. The ancient phyllosilicates in places such as this could have served as reaction centers for organic molecules. Previous experiments even suggest that phyllosilicates could have played a role in the origin of life. Regardless of whether life formed on early Mars or not, evaluating the type and thickness of clay-bearing units on Mars provides insights into plausible aqueous processes and chemical conditions both during the time of formation of the phyllosilicates, but also the subsequent period following their formation. The phyllosilicate outcrops at Mawrth Vallis extend across a broad (similar to 1000 km) region and exhibit a consistent general trend of Al-phyllosilicates and amorphous Al/Si species at the top of the clay profile and Fe/Mg-phyllosilicates on the bottom. This implies either a change in water chemistry, a change in material being altered, or an alteration profile where the upper clays were leached and altered more significantly than those below. A change in iron in the phyllosilicate units is also observed such that an Fe2+-bearing unit is frequently observed between the Fe3+- and Mg-rich phyllosilicates below and the Al/Si-rich materials above. Abrupt changes in chemistry like this are often indicative of biogeochemical activity on Earth. Possible microbe-clay interactions are considered in comparison with the CRISM observations. This study evaluates CRISM spectra from four images of different outcrops across the Mawrth Vallis region and evaluates the observed phyllosilicates and clay components in terms of plausible aqueous and microbial processes and the potential for retention of biosignatures, if present. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Bishop, Janice L.; Saper, Lee] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Bishop, Janice L.; Des Marais, David J.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Loizeau, Damien] ESA ESTEC, Noordwijk, Netherlands.
[McKeown, Nancy K.] Grant MacEwan Univ, Dept Phys Sci, Edmonton, AB T5J 4S2, Canada.
[Saper, Lee] Brown Univ, Dept Geol Sci, Providence, RI 02916 USA.
[Dyar, M. Darby] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
[Parente, Mario] Univ Massachusetts, Dept Elect & Comp Engn, Amherst, MA 01003 USA.
[Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Bishop, JL (reprint author), SETI Inst, Carl Sagan Ctr, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM jbishop@seti.org
RI Murchie, Scott/E-8030-2015
OI Murchie, Scott/0000-0002-1616-8751
FU European Space Agency; National Science Foundation; NASA Astrobiology
Institute
FX The authors thank the MRO CRISM and HiRISE science and operations teams
for acquiring the data and providing support to J. Bishop for this work.
Thanks are also due to NASA for supporting Brown University's RELAB
facility. The authors are grateful to Javier Cuadros and an anonymous
reviewer for helpful comments. Support from a research fellow grant from
the European Space Agency to D. Loizeau and from the National Science
Foundation and the NASA Astrobiology Institute to L. Saper through the
Research Experience for Undergraduates program at the SETI Institute are
greatly appreciated.
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP 15
PY 2013
VL 86
BP 130
EP 149
DI 10.1016/j.pss.2013.05.006
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 251EO
UT WOS:000326910800012
ER
PT J
AU ElShafie, A
Heggy, E
AF ElShafie, Ahmed
Heggy, Essam
TI Dielectric and hardness measurements of planetary analog rocks in
support of in-situ subsurface sampling
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Hardness; Dielectric properties; Subsurface sampling; Drilling; Mars;
Planetary surfaces
ID MARTIAN SUBSURFACE; SCHMIDT HAMMER; RADAR
AB Accurate assessment of the subsurface mechanical characteristics and how they correlate with dielectric properties is crucial to optimize future drilling and sampling investigations on planetary bodies. For 12 different types of basaltic rocks with different hardnesses, we use capacitive cells to measure the real part of the dielectric constant over the frequency range 100-1000 MHz, and a Schmidt hammer hardness tester to measure the hardness using a scale of 10-100. Our measurements suggest that the real part of the dielectric constant and rock hardness are linearly correlated. Additionally, sample hardness was linearly correlated to density. For a density ranging from 0.82 to 3.05 g/cm(3), the real part of the dielectric constant epsilon' and rebound hardness values R ranged from epsilon' =1.8-7.6 and R=14.16-68 for the different basalt samples. Hence, high dielectric constants imply a high rock hardness value and vice versa. We concluded that for volcanic surfaces that are analogous to the Martian surface as well as other planetary surfaces, there is an inverse correlation between drilling penetration rate based on the rotary-percussive drill method and the dielectric constant. Dielectric inversion from planetary radar probing experiments proposed herein is a crucial method to locate regions with lowest hardness and hence highest drilling penetration rate in desiccated volcanic planetary subsurfaces. The use of these cross-correlation measurements can optimize future drilling experiments and ensure that they reach their targets of opportunities, minimize losses in drilling performance, or the unnecessary use of power that will be needed for the continuity of the investigation. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [ElShafie, Ahmed] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA.
[Heggy, Essam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Heggy, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM heggy@jpl.nasa.gov
FU The NASA Planetary Geology and Geophysics Program [NNXZ08AKA2G,
NNG05GL11G]; Arkansas Center for Space and Planetary Sciences,
University of Arkansas; Keck Institute for Space Studies; National
Aeronautics and Space Administration
FX The authors would like to thank Dr. Valerie Ciarletti from LATMOS,
France and Dr. Stephen Clifford from the Lunar and Planetary Institute
for their helpful discussion to improve this work. The NASA Planetary
Geology and Geophysics Program supported this work under Grants
NNXZ08AKA2G and NNG05GL11G. Additional support for PhD graduate student
ElShafie was provided by the Arkansas Center for Space and Planetary
Sciences, University of Arkansas and the Keck Institute for Space
Studies. 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 25
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP 15
PY 2013
VL 86
BP 150
EP 154
DI 10.1016/j.pss.2013.02.003
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 251EO
UT WOS:000326910800013
ER
PT J
AU Mishchenko, MI
Goldstein, DH
Chowdhary, J
Lompado, A
AF Mishchenko, Michael I.
Goldstein, Dennis H.
Chowdhary, Jacek
Lompado, Arthur
TI Radiative transfer theory verified by controlled laboratory experiments
SO OPTICS LETTERS
LA English
DT Article
ID DISCRETE RANDOM-MEDIA; COHERENT BACKSCATTERING; SPHERICAL-PARTICLES;
SCATTERING
AB We report the results of high-accuracy controlled laboratory measurements of the Stokes reflection matrix for suspensions of submicrometer-sized latex particles in water and compare them with the results of a numerically exact computer solution of the vector radiative transfer equation (VRTE). The quantitative performance of the VRTE is monitored by increasing the volume packing density of the latex particles from 2% to 10%. Our results indicate that the VRTE can be applied safely to random particulate media with packing densities up to similar to 2%. VRTE results for packing densities of the order of 5% should be taken with caution, whereas the polarized bidirectional reflectivity of suspensions with larger packing densities cannot be accurately predicted. We demonstrate that a simple modification of the phase matrix entering the VRTE based on the so-called static structure factor can be a promising remedy that deserves further examination.
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Goldstein, Dennis H.; Lompado, Arthur] Polaris Sensor Technol, Huntsville, AL 35801 USA.
[Chowdhary, Jacek] Columbia Univ, Dept Appl Phys & Appl Math, 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
RI Mishchenko, Michael/D-4426-2012
FU Department of Energy [DE-SC0008285]; NASA; agency of the United States
Government
FX We appreciate useful discussions with Brian Cairns, David Chenault,
Thomas Kulp, Li Liu, and Thomas Reichardt. This material is based upon
work supported by the Department of Energy under Award Number
DE-SC0008285 managed by Victoria Franques, the NASA Remote Sensing
Theory Program managed by Lucia Tsaoussi, and the NASA Radiation
Sciences Program managed by Hal Maring. This report was prepared as an
account of work sponsored by an agency of the United States Government.
Neither the United States Government nor any agency thereof, nor any of
their employees, makes any warranty, express or implied, or assumes any
legal liability or responsibility for the accuracy, completeness, or
usefulness of any information, apparatus, product, or process disclosed,
or represents that its use would not infringe privately owned rights.
Reference herein to any specific commercial product, process, or service
by trade name, trademark, manufacturer, or otherwise does not
necessarily constitute or imply its endorsement, recommendation, or
favoring by the United States Government or any agency thereof. The
views and opinions of authors expressed herein do not necessarily state
or reflect those of the United States Government or any agency thereof.
NR 25
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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 SEP 15
PY 2013
VL 38
IS 18
BP 3522
EP 3525
DI 10.1364/OL.38.003522
PG 4
WC Optics
SC Optics
GA 228TH
UT WOS:000325212800014
PM 24104804
ER
PT J
AU Matrajt, G
Messenger, S
Joswiak, D
Brownlee, D
AF Matrajt, Graciela
Messenger, Scott
Joswiak, Dave
Brownlee, Don
TI Textures and isotopic compositions of carbonaceous materials in A and
B-type Stardust tracks: Track 130 (Bidi), track 141 (Coki) and track 80
(Tule)
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID COMET 81P/WILD 2; INTERPLANETARY DUST PARTICLES; TAGISH LAKE METEORITE;
ORGANIC-MATTER; DEUTERIUM FRACTIONATION; INFRARED-SPECTROSCOPY;
INTERSTELLAR CLOUDS; AEROGEL; SAMPLES; ORIGIN
AB We analyzed carbonaceous materials in the two main morphological types of Stardust tracks (A, and B). We analyzed 71 particles (similar to 1-10 mu m in size) distributed along these tracks with transmission electron microscopy (TEM) and found carbon associated with 16 of them. The carbonaceous materials occur in five distinct morphologies: graphitic, smooth, dirty, spongy and globular, covering most of the range of morphologies observed in primitive meteorites and interplanetary dust particles. We measured N and C isotopic compositions on 5 of these particles and found that all but one have terrestrial isotopic compositions. The anomalous particle had a moderate N-15 enrichment (delta N-15 = 150 +/- 36 parts per thousand, 2 sigma) and both globular and spongy morphologies. The carbonaceous materials are not preferentially associated with particles of a particular size but are randomly distributed in all three tracks. Published by Elsevier Ltd.
C1 [Matrajt, Graciela; Joswiak, Dave; Brownlee, Don] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Messenger, Scott] NASA, Robert M Walker Lab Space Sci, ARES, JSC, Houston, TX 77573 USA.
RP Matrajt, G (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA.
EM matrajt@astro.washington.edu
FU NASA [NNX10AI89GS01, NNG06GG00GS05]
FX This work was supported by NASA grants NNX10AI89GS01 and NNG06GG00GS05.
We wish to thank Christine Floss, Gregory Herzog and two anonymous
reviewers for their helpful comments. G.M acknowledges Nayeli
Pages-Matrajt who served as a source of inspiration for this work.
NR 68
TC 1
Z9 1
U1 1
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 SEP 15
PY 2013
VL 117
BP 65
EP 79
DI 10.1016/j.gca.2013.04.014
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 213DU
UT WOS:000324035300005
ER
PT J
AU Tompson, SR
AF Tompson, Sara R.
TI Beyond the God Particle
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Tompson, Sara R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Tompson, SR (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
NR 1
TC 0
Z9 0
U1 0
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 SEP 15
PY 2013
VL 138
IS 15
BP 101
EP 102
PG 2
WC Information Science & Library Science
SC Information Science & Library Science
GA 218OR
UT WOS:000324442500241
ER
PT J
AU Stanton, TP
Shaw, WJ
Truffer, M
Corr, HFJ
Peters, LE
Riverman, KL
Bindschadler, R
Holland, DM
Anandakrishnan, S
AF Stanton, T. P.
Shaw, W. J.
Truffer, M.
Corr, H. F. J.
Peters, L. E.
Riverman, K. L.
Bindschadler, R.
Holland, D. M.
Anandakrishnan, S.
TI Channelized Ice Melting in the Ocean Boundary Layer Beneath Pine Island
Glacier, Antarctica
SO SCIENCE
LA English
DT Article
ID WEST ANTARCTICA; SHELF; SHEET
AB Ice shelves play a key role in the mass balance of the Antarctic ice sheets by buttressing their seaward-flowing outlet glaciers; however, they are exposed to the underlying ocean and may weaken if ocean thermal forcing increases. An expedition to the ice shelf of the remote Pine Island Glacier, a major outlet of the West Antarctic Ice Sheet that has rapidly thinned and accelerated in recent decades, has been completed. Observations from geophysical surveys and long-term oceanographic instruments deployed down bore holes into the ocean cavity reveal a buoyancy-driven boundary layer within a basal channel that melts the channel apex by 0.06 meter per day, with near-zero melt rates along the flanks of the channel. A complex pattern of such channels is visible throughout the Pine Island Glacier shelf.
C1 [Stanton, T. P.; Shaw, W. J.] Naval Postgrad Sch, Dept Oceanog, Monterey, CA 93943 USA.
[Truffer, M.] Univ Alaska, Inst Geophys, Fairbanks, AK 99775 USA.
[Corr, H. F. J.] British Antarctic Survey, Cambridge CB3 OET, England.
[Peters, L. E.; Riverman, K. L.; Anandakrishnan, S.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Peters, L. E.; Riverman, K. L.; Anandakrishnan, S.] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA.
[Bindschadler, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Holland, D. M.] NYU, Dept Math, New York, NY 10012 USA.
RP Stanton, TP (reprint author), Naval Postgrad Sch, Dept Oceanog, Monterey, CA 93943 USA.
EM stanton@nps.edu
FU NSF's Office of Polar Programs under NSF [ANT-0732926]; NASA's
Cryospheric Sciences Program; New York University Abhu Dabi grant
[1204]; Natural Environment Research Council-British Antarctic Survey
Polar Science for Planet Earth Program
FX Data presented here are archived with the supplementary materials and
also as a MATLAB data structure at www.oc.nps.edu/similar to
stanton/pig/data/data.html/PIGSITE1_first35days. The authors acknowledge
the contributions of J. Stockel in software development and deployment
of the ocean instruments, D. Pomraning in designing and manning the
hot-water drill equipment, and M. Shortt for making the British
Antarctic Survey pRES field measurements. Outstanding logistic and
safety support was provided by K. Gibbon, D. Einerson, E. Steinarsson,
F. Mcarthy, S. Consalvi, the PIG support camp personnel, and the NSF
Antarctic support team. This research project was supported by NSF's
Office of Polar Programs under NSF grants including ANT-0732926, funding
from NASA's Cryospheric Sciences Program, New York University Abhu Dabi
grant 1204, and the Natural Environment Research Council-British
Antarctic Survey Polar Science for Planet Earth Program.
NR 17
TC 30
Z9 30
U1 2
U2 42
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD SEP 13
PY 2013
VL 341
IS 6151
BP 1236
EP 1239
DI 10.1126/science.1239373
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 215ZA
UT WOS:000324248800042
PM 24031016
ER
PT J
AU Kim, JW
Siochi, EJ
Carpena-Nunez, J
Wise, KE
Connell, JW
Lin, Y
Wincheski, RA
AF Kim, Jae-Woo
Siochi, Emilie J.
Carpena-Nunez, Jennifer
Wise, Kristopher E.
Connell, John W.
Lin, Yi
Wincheski, Russell A.
TI Polyaniline/Carbon Nanotube Sheet Nanocomposites: Fabrication and
Characterization
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE carbon nanotube; polyaniline; structural nanocomposites
ID SINGLE-WALL CARBON; IN-SITU POLYMERIZATION; MECHANICAL-PROPERTIES;
COMPOSITE FIBERS; STRENGTH; FILMS; REINFORCEMENT; ENHANCEMENT;
TOUGHNESS; STIFFNESS
AB Practical approaches are needed to take advantage of the nanometer-scale mechanical properties of carbon nanotubes (CNTs) at the macroscopic scale. This study was conducted to elucidate the salient factors that can maximize the mechanical properties of nanocomposites fabricated from commercially available CNT sheets. The CNT sheets were modified by stretching to improve CNT alignment and in situ polymerization using polyaniline (PANI), a pi-conjugated conductive polymer, as a binder. The resulting CNT nanocomposites were subsequently postprocessed by hot pressing and/or high temperature treatment to carbonize the PANI as a means to improve mechanical properties. The PANI/CNT nanocomposites demonstrated significant improvement in mechanical properties compared to pristine CNT sheets. The highest specific tensile strength of PANI/stretched CNT nanocomposite was 484 MPa/(g/cm(3)), which was achieved in a sample with similar to 42 wt % of PANI. This specimen was fabricated by in situ polymerization followed by hot pressing. The highest specific Young's modulus of 17.1 GPa/(g/cm(3)) was measured on a sample that was hot-pressed and carbonized. In addition, the highest DC-electrical conductivity of 621 S/cm was obtained on a sample prepared by in situ PANI on a stretched CNT sheet.
C1 [Kim, Jae-Woo; Lin, Yi] Natl Inst Aerosp, Hampton, VA 23681 USA.
[Siochi, Emilie J.; Carpena-Nunez, Jennifer; Wise, Kristopher E.; Connell, John W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
[Wincheski, Russell A.] NASA, Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23681 USA.
RP Kim, JW (reprint author), Natl Inst Aerosp, Hampton, VA 23681 USA.
EM jae-woo.kim-1@nasa.gov; j.siochi@nasa.gov
RI Kim, Jae-Woo/A-8314-2008
FU Space Technology Research Fellowship by the NASA Office of the Chief
Technologist [NNX11AN21H]
FX The authors thank Nanocomp Technologies, Inc., for supplying the
pristine CNT materials. J.C.N. acknowledges support by the Space
Technology Research Fellowship (Grant No. NNX11AN21H), provided by the
NASA Office of the Chief Technologist.
NR 44
TC 11
Z9 11
U1 3
U2 70
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 SEP 11
PY 2013
VL 5
IS 17
BP 8597
EP 8606
DI 10.1021/am402077d
PG 10
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA 294BJ
UT WOS:000330017100046
PM 23981043
ER
PT J
AU Sidick, E
AF Sidick, Erkin
TI Extended scene Shack-Hartmann wavefront sensor algorithm: minimization
of scene content dependent shift estimation errors
SO APPLIED OPTICS
LA English
DT Article
AB An adaptive periodic-correlation (APC) algorithm was developed for use in extended-scene Shack-Hartmann wavefront sensors. It provides high accuracy even when the subimages in a frame captured by a Shack-Hartmann camera are not only shifted but also distorted relative to each other. Recently we found that the shift estimate error of the APC algorithm has a component that depends on the content of the extended scene. In this paper, we assess the amount of that error and propose a method to minimize it. (c) 2013 Optical Society of America
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sidick, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Erkin.Sidick@jpl.nasa.gov
NR 9
TC 0
Z9 0
U1 1
U2 10
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
J9 APPL OPTICS
JI Appl. Optics
PD SEP 10
PY 2013
VL 52
IS 26
BP 6487
EP 6496
DI 10.1364/AO.52.006487
PG 10
WC Optics
SC Optics
GA 216VK
UT WOS:000324313200009
PM 24085124
ER
PT J
AU Giusarma, E
de Putter, R
Ho, S
Mena, O
AF Giusarma, Elena
de Putter, Roland
Ho, Shirley
Mena, Olga
TI Constraints on neutrino masses from Planck and Galaxy clustering data
SO PHYSICAL REVIEW D
LA English
DT Article
ID DIGITAL SKY SURVEY; BARYON ACOUSTIC-OSCILLATIONS; PHOTOMETRIC LUMINOUS
GALAXIES; POWER-SPECTRUM ANALYSIS; SDSS-III; DATA RELEASE; SPECTROSCOPIC
SURVEY; COSMOLOGICAL IMPLICATIONS; SYSTEMATIC UNCERTAINTIES; MASSIVE
NEUTRINOS
AB We present here bounds on neutrino masses from the combination of recent Planck cosmic microwave background (CMB) measurements and galaxy clustering information from the Baryon Oscillation Spectroscopic Survey, part of the Sloan Digital Sky Survey-III. We use the full shape of either the photometric angular clustering (Data Release 8) or the 3D spectroscopic clustering (Data Release 9) power spectrum in different cosmological scenarios. In the Lambda CDM scenario, spectroscopic galaxy clustering measurements improve significantly the existing neutrino mass bounds from Planck data. We find Sigma m(v) < 0.39 eV at 95% confidence level for the combination of the 3D power spectrum with Planck CMB data (wi lensing included) and Wilkinson Microwave Anisoptropy Probe 9-year polarization measurements. Therefore, robust neutrino mass constraints can be obtained without the addition of the prior on the Hubble constant from Hubble Space Telescope. In extended cosmological scenarios with a dark energy fluid or with nonflat geometries, galaxy clustering measurements are essential to pin down the neutrino mass bounds, providing in the majority of cases better results than those obtained from the associated measurement of the baryon acoustic oscillation scale only. In the presence of a freely varying (constant) dark energy equation of state, we find Sigma m(v) < 0.49 eV at 95% confidence level for the combination of the 3D power spectrum with Planck CMB data (with lensing included) and Wilkinson Microwave Anisoptropy Probe 9-year polarization measurements. This same data combination in nonflat geometries provides the neutrino mass bound Sigma m(v) < 0.35 eV at 95% confidence level.
C1 [Giusarma, Elena; Mena, Olga] Univ Valencia, CSIC, IFIC, Valencia 46071, Spain.
[de Putter, Roland] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[de Putter, Roland] CALTECH, Pasadena, CA 91125 USA.
[Ho, Shirley] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Dept Phys, Pittsburgh, PA 15213 USA.
RP Giusarma, E (reprint author), Univ Valencia, CSIC, IFIC, Valencia 46071, Spain.
FU National Aeronautics and Space Administration; Consolider Ingenio
Project [CSD2007-00060]; Spanish Ministry Science [FPA2011-29678]; ITN
Invisibles [PITN-GA-2011-289442]; [PROMETEO/2009/116]
FX The authors would like to thank Shun Saito for help concerning DR9 power
spectrum measurements and Maria Archidiacono for useful help with the
manuscript. Part of 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.
O.M. is supported by the Consolider Ingenio Project No. CSD2007-00060,
by PROMETEO/2009/116, by the Spanish Ministry Science Project No.
FPA2011-29678 and by the ITN Invisibles PITN-GA-2011-289442.
NR 50
TC 35
Z9 35
U1 0
U2 8
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 SEP 10
PY 2013
VL 88
IS 6
AR 063515
DI 10.1103/PhysRevD.88.063515
PG 9
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 215TR
UT WOS:000324233900002
ER
PT J
AU Pasham, DR
Strohmayer, TE
AF Pasham, Dheeraj R.
Strohmayer, Tod E.
TI CAN THE 62 DAY X-RAY PERIOD OF ULX M82 X-1 BE DUE TO A PRECESSING
ACCRETION DISK?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE black hole physics; methods: data analysis; X-rays: binaries; X-rays:
individual (M82 X-1)
ID MASS BLACK-HOLES; NGC 5408 X-1; SPECTRAL-ANALYSIS; ORBITAL PERIOD;
TIME-SERIES; BINARIES; EVOLUTION; DISCOVERY; GALAXIES; STATE
AB We have analyzed all archival Rossi X-Ray Timing Explorer/Proportional Counter Array monitoring observations of the ultraluminous X-ray source M82 X-1 in order to study the properties of its 62 day X-ray period, which was found by Kaaret and Feng in 2007. Based on its high coherence, it has been argued that the observed period is the orbital period of the binary. Utilizing a much longer data set than in previous studies, we find the following. (1) The phase-resolved X-ray (3-15 keV) spectra-modeled with a thermal accretion disk and a power law-suggest that the accretion disk's contribution to the total flux is strongly modulated with phase. (2) Suggestive evidence for a sudden phase shift of approximately 0.4 in phase (25 days) between the first and the second halves of the light curve separated by roughly 1000 days. If confirmed, the implied timescale to change the period is similar to 10 yr, which is exceptionally fast for an orbital phenomenon. These two independent pieces of evidence are consistent with the periodicity being due to a precessing accretion disk, similar to the super-orbital periods observed in systems like Her X-1, LMC X-4, and SS433. However, the timing evidence for a change in the period needs to be confirmed with additional observations. This should be possible with further monitoring of M82 with instruments such as the Swift X-Ray Telescope.
C1 [Pasham, Dheeraj R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Strohmayer, Tod E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Pasham, DR (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM dheeraj@astro.umd.edu; tod.strohmayer@nasa.gov
NR 41
TC 8
Z9 8
U1 0
U2 3
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 SEP 10
PY 2013
VL 774
IS 2
AR L16
DI 10.1088/2041-8205/774/2/L16
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 216TR
UT WOS:000324307900001
ER
PT J
AU Zhao, JW
Bogart, RS
Kosovichev, AG
Duvall, TL
Hartlep, T
AF Zhao, Junwei
Bogart, R. S.
Kosovichev, A. G.
Duvall, T. L., Jr.
Hartlep, Thomas
TI DETECTION OF EQUATORWARD MERIDIONAL FLOW AND EVIDENCE OF DOUBLE-CELL
MERIDIONAL CIRCULATION INSIDE THE SUN
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: helioseismology; Sun: interior; Sun: oscillations
ID TIME-DISTANCE HELIOSEISMOLOGY; DYNAMICS-OBSERVATORY SDO; MAGNETIC-FLUX
TRANSPORT; UPPER CONVECTION ZONE; DIFFERENTIAL ROTATION; SOLAR INTERIOR;
OSCILLATION; PROSPECTS; MODELS; IMAGER
AB Meridional flow in the solar interior plays an important role in redistributing angular momentum and transporting magnetic flux inside the Sun. Although it has long been recognized that the meridional flow is predominantly poleward at the Sun's surface and in its shallow interior, the location of the equatorward return flow and the meridional flow profile in the deeper interior remain unclear. Using the first 2 yr of continuous helioseismology observations from the Solar Dynamics Observatory/Helioseismic Magnetic Imager, we analyze travel times of acoustic waves that propagate through different depths of the solar interior carrying information about the solar interior dynamics. After removing a systematic center-to-limb effect in the helioseismic measurements and performing inversions for flow speed, we find that the poleward meridional flow of a speed of 15 m s(-1) extends in depth from the photosphere to about 0.91 R-circle dot. An equatorward flow of a speed of 10 m s(-1) is found between 0.82 and 0.91 R-circle dot in the middle of the convection zone. Our analysis also shows evidence of that the meridional flow turns poleward again below 0.82R(circle dot), indicating an existence of a second meridional circulation cell below the shallower one. This double-cell meridional circulation profile with an equatorward flow shallower than previously thought suggests a rethinking of how magnetic field is generated and redistributed inside the Sun.
C1 [Zhao, Junwei; Bogart, R. S.; Kosovichev, A. G.; Hartlep, Thomas] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Duvall, T. L., Jr.] NASA, Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zhao, JW (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
RI Zhao, Junwei/A-1177-2007;
OI Hartlep, Thomas/0000-0002-5062-9507
FU NASA [NAS5-02139]
FX We thank the two anonymous referees whose comments help to improve the
presentation and quality of this Letter. SDO is a NASA mission, and HMI
project is supported by NASA contract NAS5-02139 to Stanford University.
NR 36
TC 98
Z9 99
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 10
PY 2013
VL 774
IS 2
AR L29
DI 10.1088/2041-8205/774/2/L29
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 216TR
UT WOS:000324307900014
ER
PT J
AU Basu-Zych, AR
Lehmer, BD
Hornschemeier, AE
Goncalves, TS
Fragos, T
Heckman, TM
Overzier, RA
Ptak, AF
Schiminovich, D
AF Basu-Zych, Antara R.
Lehmer, Bret D.
Hornschemeier, Ann E.
Goncalves, Thiago S.
Fragos, Tassos
Heckman, Timothy M.
Overzier, Roderik A.
Ptak, Andrew F.
Schiminovich, David
TI EVIDENCE FOR ELEVATED X-RAY EMISSION IN LOCAL LYMAN BREAK GALAXY ANALOGS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: starburst;
X-rays: binaries
ID STAR-FORMING GALAXIES; ULTRAVIOLET-LUMINOUS GALAXIES; MASS-METALLICITY
RELATION; ACTIVE GALACTIC NUCLEI; FORMATION RATE INDICATOR; DIGITAL SKY
SURVEY; FIELD-NORTH SURVEY; METAL-POOR STARS; DEEP FIELD; STELLAR MASS
AB Our knowledge of how X-ray emission scales with star formation at the earliest times in the universe relies on studies of very distant Lyman break galaxies (LBGs). In this paper, we study the relationship between the 2-10 keV X-ray luminosity (L-X), assumed to originate from X-ray binaries (XRBs), and star formation rate (SFR) in ultraviolet (UV) selected z < 0.1 Lyman break analogs (LBAs). We present Chandra observations for four new Galaxy Evolution Explorer selected LBAs. Including previously studied LBAs, Haro 11 and VV 114, we find that LBAs demonstrate L-X/SFR ratios that are elevated by similar to 1.5 sigma compared to local galaxies, similar to the ratios found for stacked LBGs in the early universe (z > 2). Unlike some of the composite LBAs studied previously, we show that these LBAs are unlikely to harbor active galactic nuclei, based on their optical and X-ray spectra and the spatial distribution of the X-rays in three spatially extended cases. Instead, we expect that high-mass X-ray binaries (HMXBs) dominate the X-ray emission in these galaxies, based on their high specific SFRs (sSFRs SFR/M-star >= 10(-9) yr(-1)), which suggest the prevalence of young stellar populations. Since both UV-selected populations (LBGs and LBAs) have lower dust attenuations and metallicities compared to similar samples of more typical local galaxies, we investigate the effects of dust extinction and metallicity on the L-X/SFR for the broader population of galaxies with high sSFRs (>10(-10) yr(-1)). The estimated dust extinctions (corresponding to column densities of N-H < 10(22) cm(-2)) are expected to have insignificant effects on observed L-X/SFR ratio for the majority of galaxy samples. We find that the observed relationship between L-X/SFR and metallicity appears consistent with theoretical expectations from XRB population synthesis models. Therefore, we conclude that lower metallicities, related to more luminous HMXBs such as ultraluminous X-ray sources, drive the elevated L-X/SFR observed in our sample of z < 0.1 LBAs. The relatively metal-poor, active mode of star formation in LBAs and distant z > 2 LBGs may yield higher total HMXB luminosity than found in typical galaxies in the local universe.
C1 [Basu-Zych, Antara R.; Lehmer, Bret D.; Hornschemeier, Ann E.; Ptak, Andrew F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lehmer, Bret D.; Hornschemeier, Ann E.; Heckman, Timothy M.; Ptak, Andrew F.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Goncalves, Thiago S.] Univ Fed Rio de Janeiro, Observ Valongo, BR-22240060 Rio De Janeiro, RJ, Brazil.
[Fragos, Tassos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Overzier, Roderik A.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Overzier, Roderik A.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA.
RP Basu-Zych, AR (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
EM antara.r.basu-zych@nasa.gov
RI Fragos, Tassos/A-3581-2016
OI Fragos, Tassos/0000-0003-1474-1523
FU Chandra Cycle 12 program [12620841]; CfA; ITC prize fellowship programs;
National Aeronautics and Space Administration
FX This research was supported by Chandra Cycle 12 program No. 12620841
(PI: Basu-Zych). We thank our anonymous referee for helpful suggestions,
A. Prestwich for sharing her work on ULXs in extremely low metallicity
galaxies, S. Mineo for providing useful comparison data, and J. Mullaney
for sharing his IR code. The author gratefully acknowledges B. D.
Johnson, A. Henry, and V. Antoniou for helpful discussions. T.F.
acknowledges support from CfA and ITC prize fellowship programs. 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.
NR 100
TC 24
Z9 24
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2013
VL 774
IS 2
AR 152
DI 10.1088/0004-637X/774/2/152
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211EW
UT WOS:000323888900061
ER
PT J
AU Deming, D
Wilkins, A
McCullough, P
Burrows, A
Fortney, JJ
Agol, E
Dobbs-Dixon, I
Madhusudhan, N
Crouzet, N
Desert, JM
Gilliland, RL
Haynes, K
Knutson, HA
Line, M
Magic, Z
Mandell, AM
Ranjan, S
Charbonneau, D
Clampin, M
Seager, S
Showman, AP
AF Deming, Drake
Wilkins, Ashlee
McCullough, Peter
Burrows, Adam
Fortney, Jonathan J.
Agol, Eric
Dobbs-Dixon, Ian
Madhusudhan, Nikku
Crouzet, Nicolas
Desert, Jean-Michel
Gilliland, Ronald L.
Haynes, Korey
Knutson, Heather A.
Line, Michael
Magic, Zazralt
Mandell, Avi M.
Ranjan, Sukrit
Charbonneau, David
Clampin, Mark
Seager, Sara
Showman, Adam P.
TI INFRARED TRANSMISSION SPECTROSCOPY OF THE EXOPLANETS HD 209458b AND
XO-1b USING THE WIDE FIELD CAMERA-3 ON THE HUBBLE SPACE TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planets and satellites: atmospheres; techniques:
photometric; techniques: spectroscopic
ID TRANSITING PLANET ATMOSPHERES; HOT-JUPITER XO-1B; EXTRASOLAR PLANET; GJ
1214B; ABSORPTION FEATURES; CIRCULATION MODELS; SUPER-EARTHS; SPECTRUM;
189733B; WATER
AB Exoplanetary transmission spectroscopy in the near-infrared using the Hubble Space Telescope (HST) NICMOS is currently ambiguous because different observational groups claim different results from the same data, depending on their analysis methodologies. Spatial scanning with HST/WFC3 provides an opportunity to resolve this ambiguity. We here report WFC3 spectroscopy of the giant planets HD 209458b and XO-1b in transit, using spatial scanning mode for maximum photon-collecting efficiency. We introduce an analysis technique that derives the exoplanetary transmission spectrum without the necessity of explicitly decorrelating instrumental effects, and achieves nearly photon-limited precision even at the high flux levels collected in spatial scan mode. Our errors are within 6% (XO-1) and 26% (HD 209458b) of the photon-limit at a resolving power of lambda/delta lambda similar to 70, and are better than 0.01% per spectral channel. Both planets exhibit water absorption of approximately 200 ppm at the water peak near 1.38 mu m. Our result for XO-1b contradicts the much larger absorption derived from NICMOS spectroscopy. The weak water absorption we measure for HD209458b is reminiscent of the weakness of sodium absorption in the first transmission spectroscopy of an exoplanet atmosphere by Charbonneau et al. Model atmospheres having uniformly distributed extra opacity of 0.012 cm(2) g(-1) account approximately for both our water measurement and the sodium absorption. Our results for HD 209458b support the picture advocated by Pont et al. in which weak molecular absorptions are superposed on a transmission spectrum that is dominated by continuous opacity due to haze and/or dust. However, the extra opacity needed for HD 209458b is grayer than for HD 189733b, with a weaker Rayleigh component.
C1 [Deming, Drake; Wilkins, Ashlee] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[McCullough, Peter; Crouzet, Nicolas] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Agol, Eric; Dobbs-Dixon, Ian] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Madhusudhan, Nikku] Yale Univ, Yale Ctr Astron Astrophys, New Haven, CT 06511 USA.
[Desert, Jean-Michel; Knutson, Heather A.; Line, Michael] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Haynes, Korey] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA.
[Haynes, Korey; Mandell, Avi M.; Clampin, Mark] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Magic, Zazralt] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Magic, Zazralt] Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Ranjan, Sukrit; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Deming, D (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM ddeming@astro.umd.edu
OI Dobbs-Dixon, Ian/0000-0002-4989-6501; Fortney,
Jonathan/0000-0002-9843-4354; Ranjan, Sukrit/0000-0002-5147-9053;
/0000-0002-0802-9145
NR 75
TC 110
Z9 111
U1 5
U2 26
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 SEP 10
PY 2013
VL 774
IS 2
AR 95
DI 10.1088/0004-637X/774/2/95
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211EW
UT WOS:000323888900004
ER
PT J
AU Eichner, T
Seitz, S
Suyu, SH
Halkola, A
Umetsu, K
Zitrin, A
Coe, D
Monna, A
Rosati, P
Grillo, C
Balestra, I
Postman, M
Koekemoer, A
Zheng, W
Host, O
Lemze, D
Broadhurst, T
Moustakas, L
Bradley, L
Molino, A
Nonino, M
Mercurio, A
Scodeggio, M
Bartelmann, M
Benitez, N
Bouwens, R
Donahue, M
Infante, L
Jouvel, S
Kelson, D
Lahav, O
Medezinski, E
Melchior, P
Merten, J
Riess, A
AF Eichner, Thomas
Seitz, Stella
Suyu, Sherry H.
Halkola, Aleksi
Umetsu, Keiichi
Zitrin, Adi
Coe, Dan
Monna, Anna
Rosati, Piero
Grillo, Claudio
Balestra, Italo
Postman, Marc
Koekemoer, Anton
Zheng, Wei
Host, Ole
Lemze, Doron
Broadhurst, Tom
Moustakas, Leonidas
Bradley, Larry
Molino, Alberto
Nonino, Mario
Mercurio, Amata
Scodeggio, Marco
Bartelmann, Matthias
Benitez, Narciso
Bouwens, Rychard
Donahue, Megan
Infante, Leopoldo
Jouvel, Stephanie
Kelson, Daniel
Lahav, Ofer
Medezinski, Elinor
Melchior, Peter
Merten, Julian
Riess, Adam
TI GALAXY HALO TRUNCATION AND GIANT ARC SURFACE BRIGHTNESS RECONSTRUCTION
IN THE CLUSTER MACSJ1206.2-0847
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (MACSJ1206.2-0847); galaxies: elliptical
and lenticular, cD; galaxies: halos; galaxies: interactions;
gravitational lensing: strong
ID DARK-MATTER HALOS; STRONG-LENSING ANALYSIS; HIGH-DENSITY ENVIRONMENTS;
FABER-JACKSON RELATION; STAR-FORMING GALAXIES; DEEP ADVANCED CAMERA;
DIGITAL SKY SURVEY; TO-LIGHT RATIOS; ELLIPTIC GALAXIES;
MASS-DISTRIBUTION
AB In this work, we analyze the mass distribution of MACSJ1206.2-0847, particularly focusing on the halo properties of its cluster members. The cluster appears relaxed in its X-ray emission, but has a significant amount of intracluster light that is not centrally concentrated, suggesting that galaxy-scale interactions are still ongoing despite the overall relaxed state. The cluster lenses 12 background galaxies into multiple images and one galaxy at z = 1.033 into a giant arc and its counterimage. The multiple image positions and the surface brightness (SFB) distribution of the arc, which is bent around several cluster members, are sensitive to the cluster galaxy halo properties. We model the cluster mass distribution with a Navarro-Frenk-White profile and the galaxy halos with two parameters for the mass normalization and the extent of a reference halo assuming scalings with their observed near-infrared light. We match the multiple image positions at an rms level of 0 ''.85 and can reconstruct the SFB distribution of the arc in several filters to a remarkable accuracy based on this cluster model. The length scale where the enclosed galaxy halo mass is best constrained is about 5 effective radii-a scale in between those accessible to dynamical and field strong-lensing mass estimates on the one hand and galaxy-galaxy weak-lensing results on the other hand. The velocity dispersion and halo size of a galaxy with m(160W),(AB) = 19.2 and M-B,M-Vega = -20.7 are sigma = 150 km s(-1) and r approximate to 26 +/- 6 kpc, respectively, indicating that the halos of the cluster galaxies are tidally stripped. We also reconstruct the unlensed source, which is smaller by a factor of similar to 5.8 in area, demonstrating the increase in morphological information due to lensing. We conclude that this galaxy likely has star-forming spiral arms with a red (older) central component.
C1 [Eichner, Thomas; Seitz, Stella; Monna, Anna] Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Eichner, Thomas; Seitz, Stella; Monna, Anna; Balestra, Italo] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Suyu, Sherry H.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Suyu, Sherry H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Moffett Field, CA 94035 USA.
[Suyu, Sherry H.; Umetsu, Keiichi] Acad Sin, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Halkola, Aleksi] Univ Lubeck, Inst Med Engn, D-23562 Lubeck, Germany.
[Zitrin, Adi; Bartelmann, Matthias] ZAH, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Coe, Dan; Postman, Marc; Koekemoer, Anton; Bradley, Larry] Space Telescope Sci Inst, Baltimore, MD 21208 USA.
[Rosati, Piero] ESO European So Observ, D-85748 Garching, Germany.
[Grillo, Claudio; Host, Ole] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Zheng, Wei; Lemze, Doron; Medezinski, Elinor; Riess, Adam] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Broadhurst, Tom] Univ Basque Country, Dept Theoret Phys, Bilbao, Spain.
CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nonino, Mario] Inst Astrofis Andalucia CSIC, E-18008 Granada, Spain.
[Mercurio, Amata] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy.
[Scodeggio, Marco] INAF IASF Milano, I-20133 Milan, Italy.
[Bouwens, Rychard] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Infante, Leopoldo] Pontificia Univ Catolica Chile, Dept Astronoia & Astrofis, Santiago De Compostela 22, Spain.
[Jouvel, Stephanie] UCL, Dept Phys & Astron, London WCIE 6 BT, England.
[Jouvel, Stephanie] Inst Cincies Espai IEEC CSIC, Bellaterra, Barcelona, Spain.
[Kelson, Daniel] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Melchior, Peter] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA.
[Melchior, Peter] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
RP Eichner, T (reprint author), Univ Sternwarte Munchen, D-81679 Munich, Germany.
RI Bartelmann, Matthias/A-5336-2014; Molino Benito, Alberto/F-5298-2014;
Grillo, Claudio/E-6223-2015;
OI Benitez, Narciso/0000-0002-0403-7455; Grillo,
Claudio/0000-0002-5926-7143; Nonino, Mario/0000-0001-6342-9662;
Balestra, Italo/0000-0001-9660-894X; Scodeggio,
Marco/0000-0002-2282-5850; Koekemoer, Anton/0000-0002-6610-2048; Umetsu,
Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360
FU Transregional Collaborative Research Centre-The Dark Universe [TRR 33];
DFG cluster of excellence "Origin and Structure of the Universe"; NASA
[NAS 5-26555]; National Science Council of Taiwan
[NSC100-2112-M-001-008-MY3]; Academia Sinica; contract research
"Internationale Spitzenforschung II-1" of the Baden Wurttemberg
Stiftung; DNRF; [186.A-0798]
FX This work is supported by the Transregional Collaborative Research
Centre TRR 33-The Dark Universe and the DFG cluster of excellence
"Origin and Structure of the Universe." We thank Jens Thomas, Ralf
Bender, and Roberto P. Saglia for fruitful discussions of the properties
of early-type galaxies. We thank the anonymous referee for his/her
comments and suggestions to improve the text. Based on observations made
with the NASA/ESA Hubble Space Telescope, obtained from the data archive
at the Space Telescope Science Institute. STScI is operated by the
Association of Universities for Research in Astronomy, Inc. under NASA
contract NAS 5-26555. The CLASH Multi-Cycle Treasury Program (GO-12065)
is based on observations made with the NASA/ESA Hubble Space Telescope.
The Space Telescope Science Institute is operated by the Association of
Universities for Research in Astronomy, Inc. under NASA contract NAS
5-26555. Part of this work is based on data collected at the Very Large
Telescope at the ESO Paranal Observatory, under Program ID 186.A-0798.
K.U. acknowledges partial support from the National Science Council of
Taiwan grant NSC100-2112-M-001-008-MY3 and from the Academia Sinica
Career Development Award. A.Z. is supported by contract research
"Internationale Spitzenforschung II-1" of the Baden Wurttemberg
Stiftung. The Dark Cosmology Centre is funded by the DNRF.
NR 97
TC 12
Z9 12
U1 1
U2 16
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2013
VL 774
IS 2
AR 774
DI 10.1088/0004-637X/774/2/124
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211EW
UT WOS:000323888900033
ER
PT J
AU Goldsmith, PF
AF Goldsmith, Paul F.
TI DIFFUSE MOLECULAR CLOUD DENSITIES FROM UV MEASUREMENTS OF CO ABSORPTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: molecules; radio lines: ISM
ID FINE-STRUCTURE EXCITATIONS; GALACTIC PLANE SURVEY;
ROTATIONAL-EXCITATION; CARBON-MONOXIDE; INTERSTELLAR CLOUDS; THERMAL
PRESSURES; COLLISIONAL EXCITATION; ULTRAVIOLET SURVEY; GAS; HYDROGEN
AB We use UV measurements of interstellar CO toward nearby stars to calculate the density in the diffuse molecular clouds containing the molecules responsible for the observed absorption. Chemical models and recent calculations of the excitation rate coefficients indicate that the regions in which CO is found have hydrogen predominantly in molecular form and that collisional excitation is by collisions with H-2 molecules. We carry out statistical equilibrium calculations using CO-H-2 collision rates to solve for the H-2 density in the observed sources without including effects of radiative trapping. We have assumed kinetic temperatures of 50 K and 100 K, finding this choice to make relatively little difference to the lowest transition. For the sources having T-10(ex) only for which we could determine upper and lower density limits, we find < n(H-2)> = 49 cm(-3). While we can find a consistent density range for a good fraction of the sources having either two or three values of the excitation temperature, there is a suggestion that the higher-J transitions are sampling clouds or regions within diffuse molecular cloud material that have higher densities than the material sampled by the J = 1-0 transition. The assumed kinetic temperature and derived H-2 density are anticorrelated when the J = 2-1 transition data, the J = 3-2 transition data, or both are included. For sources with either two or three values of the excitation temperature, we find average values of the midpoint of the density range that is consistent with all of the observations equal to 68 cm(-3) for T-k = 100 K and 92 cm(-3) for T-k = 50 K. The data for this set of sources imply that diffuse molecular clouds are characterized by an average thermal pressure between 4600 and 6800 K cm(-3).
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Goldsmith, PF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Goldsmith, Paul/H-3159-2016
NR 47
TC 11
Z9 11
U1 1
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2013
VL 774
IS 2
AR 134
DI 10.1088/0004-637X/774/2/134
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211EW
UT WOS:000323888900043
ER
PT J
AU Grondin, MH
Romani, RW
Lemoine-Goumard, M
Guillemot, L
Harding, AK
Reposeur, T
AF Grondin, M. -H.
Romani, R. W.
Lemoine-Goumard, M.
Guillemot, L.
Harding, A. K.
Reposeur, T.
TI THE VELA-X PULSAR WIND NEBULA REVISITED WITH FOUR YEARS OF FERMI LARGE
AREA TELESCOPE OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: general; ISM: individual objects (Vela-X); pulsars: general;
pulsars: individual (Vela, PSR J0835-4510)
ID GAMMA-RAY OBSERVATIONS; SUPERNOVA REMNANT; SYNCHROTRON NEBULA; WMAP
OBSERVATIONS; HESS J1825-137; EGRET DATA; EMISSION; LAT; RADIO;
EVOLUTION
AB The Vela supernova remnant (SNR) is the closest SNR to Earth containing an active pulsar, the Vela pulsar (PSR B0833-45). This pulsar is an archetype of the middle-aged pulsar class and powers a bright pulsar wind nebula (PWN), Vela-X, spanning a region of 2 degrees x 3 degrees south of the pulsar and observed in the radio, X-ray, and very high energy gamma-ray domains. The detection of the Vela-X PWN by the Fermi Large Area Telescope (LAT) was reported in the first year of the mission. Subsequently, we have reinvestigated this complex region and performed a detailed morphological and spectral analysis of this source using 4 yr of Fermi-LAT observations. This study lowers the threshold for morphological analysis of the nebula from 0.8 GeV to 0.3 GeV, allowing for the inspection of distinct energy bands by the LAT for the first time. We describe the recent results obtained on this PWN and discuss the origin of the newly detected spatial features.
C1 [Grondin, M. -H.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Romani, R. W.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Romani, R. W.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Lemoine-Goumard, M.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Guillemot, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Harding, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Grondin, MH (reprint author), IRAP, CNRS, F-31028 Toulouse 4, France.
EM mgrondin@irap.omp.eu
FU Alexander von Humboldt Foundation (Germany); Centre National d'Etudes
Spatiales (CNES, France)
FX M. H. G. acknowledges support from the Alexander von Humboldt Foundation
(Germany) and from the Centre National d'Etudes Spatiales (CNES,
France). M. H. G. thanks Felix A. Aharonian and Patrick O. Slane for
helpful comments and discussions.
NR 53
TC 7
Z9 7
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2013
VL 774
IS 2
AR 110
DI 10.1088/0004-637X/774/2/110
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211EW
UT WOS:000323888900019
ER
PT J
AU Khangulyan, DV
Barkov, MV
Bosch-Ramon, V
Aharonian, FA
Dorodnitsyn, AV
AF Khangulyan, D. V.
Barkov, M. V.
Bosch-Ramon, V.
Aharonian, F. A.
Dorodnitsyn, A. V.
TI STAR-JET INTERACTIONS AND GAMMA-RAY OUTBURSTS FROM 3C454.3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: jets; gamma rays: galaxies; radiation mechanisms: non-thermal
ID ACTIVE GALACTIC NUCLEI; BLAZAR 3C 454.3; SPACE-TELESCOPE OBSERVATIONS;
MAGNETIC ACCELERATION; AGN JETS; HYDRODYNAMICAL MODEL; 2010 NOVEMBER;
RADIO-SOURCES; BLACK-HOLES; TORUS WIND
AB We propose a model to explain the ultra-bright GeV gamma-ray flares observed from the blazar 3C454.3. The model is based on the concept of a relativistic jet interacting with compact gas condensations produced when a star (a red giant) crosses the jet close to the central black hole. The study includes an analytical treatment of the evolution of the envelope lost by the star within the jet, and calculations of the related high-energy radiation. The model readily explains the day-long that varies on timescales of hours, GeV gamma-ray flare from 3C454.3, observed during 2010 November on top of a plateau lasting weeks. In the proposed scenario, the plateau state is caused by a strong wind generated by the heating of the stellar atmosphere due to nonthermal particles accelerated at the jet-star interaction region. The flare itself could be produced by a few clouds of matter lost by the red giant after the initial impact of the jet. In the framework of the proposed scenario, the observations constrain the key model parameters of the source, including the mass of the central black hole: M-BH similar or equal to 10(9) M-circle dot, the total jet power: L-j similar or equal to 10(48) erg s(-1), and the Doppler factor of the gamma-ray emitting clouds: delta similar or equal to 20. Whereas we do not specify the particle acceleration mechanisms, the potential gamma-ray production processes are discussed and compared in the context of the proposed model. We argue that synchrotron radiation of protons has certain advantages compared to other radiation channels of directlyaccelerated electrons. An injected proton distribution proportional to E-1 or harder below the relevant energies would be favored to alleviate the tight energetic constraints and to avoid the violation of the observational low-energy constraints.
C1 [Khangulyan, D. V.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Barkov, M. V.; Aharonian, F. A.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Barkov, M. V.] RAS, Space Res Inst, Moscow 117997, Russia.
[Bosch-Ramon, V.] Univ Barcelona IEEC UB, ICC, Dept Astron & Meteorol, E-08028 Barcelona, Spain.
[Aharonian, F. A.] Dublin Inst Adv Studies, Dublin 2, Ireland.
[Dorodnitsyn, A. V.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
[Dorodnitsyn, A. V.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA.
RP Khangulyan, DV (reprint author), JAXA, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
FU European Union [PIEF-GA-2009-252463]; Spanish Ministerio de Ciencia e
Innovacion (MICINN) [AYA2010-21782-C03-01, FPA2010-22056-C06-02];
MINECO; Marie Curie Career Integration Grant [321520]; RFBR
[12-02-01336-a]; appointment at the NASA Goddard Space Flight Center;
NASA [10-ATP10-0171]
FX The authors are thankful to S. Kelner for useful discussions and Benoit
Lott for providing observational data. The research leading to these
results has received funding from the European Union Seventh Framework
Program (FP7/2007-2013) under grant agreement PIEF-GA-2009-252463.
V.B.-R. acknowledges support by the Spanish Ministerio de Ciencia e
Innovacion (MICINN) under grants AYA2010-21782-C03-01 and
FPA2010-22056-C06-02. V.B.-R. acknowledges financial support from MINECO
through a Ramon y Cajal fellowship. This research has been supported by
the Marie Curie Career Integration Grant 321520. M. V. B. acknowledges
partial support by RFBR grant 12-02-01336-a. A. V. D. was supported by
an appointment at the NASA Goddard Space Flight Center, administered by
CRESST/UMD through a contract with NASA, and by grants from the NASA
Astrophysics Theory Program 10-ATP10-0171.
NR 52
TC 9
Z9 9
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2013
VL 774
IS 2
AR 113
DI 10.1088/0004-637X/774/2/113
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211EW
UT WOS:000323888900022
ER
PT J
AU McCormick, A
Veilleux, S
Rupke, DSN
AF McCormick, Alexander
Veilleux, Sylvain
Rupke, David S. N.
TI DUSTY WINDS: EXTRAPLANAR POLYCYCLIC AROMATIC HYDROCARBON FEATURES OF
NEARBY GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: star formation; galaxies: structure; infrared: galaxies;
intergalactic medium; ISM: jets and outflows
ID X-RAY-EMISSION; ULTRALUMINOUS INFRARED GALAXIES; DIFFUSE IONIZED-GAS; ON
SPIRAL GALAXIES; STAR-FORMING DISK; SPITZER-SPACE-TELESCOPE; ACTIVE
GALACTIC NUCLEI; LARGE-SCALE OUTFLOWS; EDGE-ON; STARBURST GALAXIES
AB Recent observations have shown the presence of dust and molecular material in galactic winds, but relatively little is known about the distribution of these outflow components. To shed some light on this issue, we have used IRAC images from the Spitzer Space Telescope archive to investigate polycyclic aromatic hydrocarbon (PAH) emission from a sample of 16 local galaxies with known winds. Our focus on nearby sources (median distance 8.6 Mpc) has revealed detailed PAH structure in the winds and allowed us to measure extraplanar PAH emission. We have identified extraplanar PAH features on scales of similar to 0.8-6.0 kpc. We find a nearly linear correlation between the amount of extraplanar PAH emission and the total infrared flux, a proxy for star formation activity in the disk. Our results also indicate a correlation between the height of extraplanar PAH emission and star formation rate surface density, which supports the idea of a surface density threshold on the energy or momentum injection rate for producing detectable extraplanar wind material.
C1 [McCormick, Alexander; Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Veilleux, Sylvain] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Veilleux, Sylvain] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Veilleux, Sylvain] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Rupke, David S. N.] Rhodes Coll, Memphis, TN 38112 USA.
RP McCormick, A (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM alexm@astro.umd.edu; veilleux@astro.umd.edu; rupked@rhodes.edu
FU NASA; NASA through Spitzer archival grant [1310149]; NSF through AST/EXC
[AST10009583]; Senior NPP Award at the NASA Goddard Space Flight Center;
Humbolt Foundation
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. Support
for this work was provided by NASA through Spitzer archival grant
1310149 and NSF through AST/EXC grant AST10009583. S.V. also
acknowledges partial support from a Senior NPP Award held at the NASA
Goddard Space Flight Center and from the Humbolt Foundation to provide
funds for a long-term visit at MPE in 2012. We acknowledge the helpful
comments of the referee. We thank Massimo Ricotti and Stacy McGaugh for
comments on an early version of the manuscript, Michael McDonald for his
suggestions regarding our electronic banding removal algorithm and his
help with "asinh" scaled images, Alberto Bolatto for his advice
regarding scale height determination, and Jonathan Fraine for his help
with coding in PyRAF. We also thank G. Bicknell, J. Bland-Hawthorn, J.
Cooper, C. Engelbracht, M. Regan, and R. Sutherland, who were co-Is on
the original Spitzer archival proposal.
NR 132
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U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2013
VL 774
IS 2
AR 126
DI 10.1088/0004-637X/774/2/126
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211EW
UT WOS:000323888900035
ER
PT J
AU Tzanavaris, P
Fragos, T
Tremmel, M
Jenkins, L
Zezas, A
Lehmer, BD
Hornschemeier, A
Kalogera, V
Ptak, A
Basu-Zych, AR
AF Tzanavaris, P.
Fragos, T.
Tremmel, M.
Jenkins, L.
Zezas, A.
Lehmer, B. D.
Hornschemeier, A.
Kalogera, V.
Ptak, A.
Basu-Zych, A. R.
TI MODELING X-RAY BINARY EVOLUTION IN NORMAL GALAXIES: INSIGHTS FROM SINGS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; galaxies: spiral; stars: evolution; X-rays: binaries
ID STAR-FORMATION RATE; BLACK-HOLE BINARIES; CHANDRA MONITORING
OBSERVATIONS; FORMATION RATE INDICATOR; INITIAL MASS FUNCTION; LOCAL
VOLUME SURVEY; SOLAR-TYPE STARS; LUMINOSITY FUNCTION; POPULATION
SYNTHESIS; ELLIPTIC GALAXIES
AB We present the largest-scale comparison to date between observed extragalactic X-ray binary (XRB) populations and theoretical models of their production. We construct observational X-ray luminosity functions (oXLFs) using Chandra observations of 12 late-type galaxies from the Spitzer Infrared Nearby Galaxy Survey. For each galaxy, we obtain theoretical XLFs (tXLFs) by combining XRB synthetic models, constructed with the population synthesis code StarTrack, with observational star formation histories (SFHs). We identify highest-likelihood models both for individual galaxies and globally, averaged over the full galaxy sample. Individual tXLFs successfully reproduce about half of the oXLFs, but for some galaxies we are unable to find underlying source populations, indicating that galaxy SFHs and metallicities are not well matched and/or that XRB modeling requires calibration on larger observational samples. Given these limitations, we find that the best models are consistent with a product of common envelope ejection efficiency and central donor concentration similar or equal to 0.1, and a 50% uniform-50% "twins" initial mass-ratio distribution. We present and discuss constituent subpopulations of tXLFs according to donor, accretor, and stellar population characteristics. The galaxy-wide X-ray luminosity due to low-mass and high-mass XRBs, estimated via our best global model tXLF, follows the general trend expected from the L-X-star formation rate and L-X-stellar mass relations of Lehmer et al. Our best models are also in agreement with modeling of the evolution of both XRBs over cosmic time and of the galaxy X-ray luminosity with redshift.
C1 [Tzanavaris, P.; Jenkins, L.; Lehmer, B. D.; Hornschemeier, A.; Ptak, A.; Basu-Zych, A. R.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA.
[Tzanavaris, P.; Lehmer, B. D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Fragos, T.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA.
[Tremmel, M.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece.
[Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece.
[Kalogera, V.] Northwestern Univ, Ctr Interdisciplinary Res & Explorat Astrophys, Evanston, IL 60208 USA.
[Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
RP Tzanavaris, P (reprint author), NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Mail Code 662, Greenbelt, MD 20771 USA.
RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016
OI Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523
FU NASA at NASA Goddard Space Flight Center; NASA [ADAP 09-ADP09-0071];
MSHE [N203404939]
FX We thank Stephan Noll for providing star formation histories from SED
fitting with CIGALE for the galaxies in this sample. We thank Chris
Belczynski for making StarTrack available to us. P.T. acknowledges
support through a NASA Postdoctoral Program Fellowship at NASA Goddard
Space Flight Center, administered by Oak Ridge Associated Universities
through a contract with NASA. T.F. is a CfA and ITC prize fellow. B.D.L.
thanks the Einstein Fellowship Program. K.B. acknowledges support from
MSHE grant N203404939. A.H., P.T., A.Z., and V.K. were also supported by
NASA ADAP 09-ADP09-0071 (PI: Hornschemeier). Computational 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 and by the Northwestern University Quest High
Performance Computing (HPC) cluster.
NR 97
TC 8
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U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2013
VL 774
IS 2
AR 136
DI 10.1088/0004-637X/774/2/136
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211EW
UT WOS:000323888900045
ER
PT J
AU Whittet, DCB
Poteet, CA
Chiar, JE
Pagani, L
Bajaj, VM
Horne, D
Shenoy, SS
Adamson, AJ
AF Whittet, D. C. B.
Poteet, C. A.
Chiar, J. E.
Pagani, L.
Bajaj, V. M.
Horne, D.
Shenoy, S. S.
Adamson, A. J.
TI ICE AND DUST IN THE PRESTELLAR DARK CLOUD LYNDS 183: PREPLANETARY MATTER
AT THE LOWEST TEMPERATURES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; dust, extinction; infrared: ISM; ISM: individual objects
(LDN 183); ISM: lines and bands; ISM: molecules
ID SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; SPECTROSCOPIC SURVEY;
MOLECULAR CLOUDS; INFRARED SPECTROGRAPH; INTERSTELLAR-MEDIUM; SOLID CO;
TAURUS; STARS; L183
AB Dust grains are nucleation centers and catalysts for the growth of icy mantles in quiescent interstellar clouds, the products of which may accumulate into preplanetary matter when new stars and solar systems form within the clouds. In this paper, we present the first spectroscopic detections of silicate dust and the molecular ices H2O, CO, and CO2 in the vicinity of the prestellar core L183 (L134N). An infrared photometric survey of the cloud was used to identify reddened background stars, and we present spectra covering solid-state absorption features in the wavelength range 2-20 mu m for nine of them. The mean composition of the ices in the best-studied line of sight (toward J15542044-0254073) is H2O:CO:CO2 approximate to 100:40:24. The ices are amorphous in structure, indicating that they have been maintained at low temperature (less than or similar to 15 K) since formation. The ice column density N(H2O) correlates with reddening by dust, exhibiting a threshold effect that corresponds to the transition from unmantled grains in the outer layers of the cloud to ice-mantled grains within, analogous to that observed in other dark clouds. A comparison of results for L183 and the Taurus and IC 5146 dark clouds suggests common behavior, with mantles first appearing in each case at a dust column corresponding to a peak optical depth iota(9.7) = 0.15 +/- 0.03 in the silicate feature. Our results support a previous conclusion that the color excess EJ-K does not obey a simple linear correlation with the total dust column in lines of sight that intercept dense clouds. The most likely explanation is a systematic change in the optical properties of the dust as the density increases.
C1 [Whittet, D. C. B.; Poteet, C. A.; Bajaj, V. M.; Horne, D.] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA.
[Whittet, D. C. B.; Poteet, C. A.; Bajaj, V. M.; Horne, D.] Rensselaer Polytech Inst, New York Ctr Astrobiol, Troy, NY 12180 USA.
[Chiar, J. E.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
[Pagani, L.] Observ Paris, CNRS, UMR 8112, LERMA, F-75014 Paris, France.
[Shenoy, S. S.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Adamson, A. J.] Southern Operat Ctr, Gemini Observ, La Serena, Chile.
RP Whittet, DCB (reprint author), Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, 110 8th St, Troy, NY 12180 USA.
OI adamson, andrew/0000-0003-1120-5178; Whittet,
Douglas/0000-0001-8539-3891
FU NASA; National Science Foundation; Cornell Atlas of Spitzer/IRS Sources
(CASSIS), a product of the Infrared Science Center at Cornell
University; JPL; NASA from the JPL/Caltech Spitzer General Observer
Program; NASA Exobiology and Evolutionary Biology program; NASA
Astrobiology Institute
FX This research has made use of observations from Spitzer Space Telescope
and data from the NASA/IPAC Infrared Science Archive, which are operated
by the Jet Propulsion Laboratory (JPL) and the California Institute of
Technology under contract with NASA. It has also made use of
observations obtained with the Infrared Telescope Facility, operated by
the University of Hawaii under a Cooperative Agreement with the NASA
Science Mission Directorate, Planetary Astronomy Program, and with the
United Kingdom Infrared Telescope, formerly operated by the Joint
Astronomy Centre on behalf of the Science and Technology Facilities
Council of the UK. This research has also made use of data products from
the Two Micron All Sky Survey, a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center (IPAC),
California Institute of Technology, funded by NASA and the National
Science Foundation, and from the Cornell Atlas of Spitzer/IRS Sources
(CASSIS), a product of the Infrared Science Center at Cornell
University, also supported by NASA and JPL. Funding for this research
was provided by NASA through awards to Rensselaer Polytechnic Institute
from the JPL/Caltech Spitzer General Observer Program, the NASA
Exobiology and Evolutionary Biology program, and the NASA Astrobiology
Institute. We are grateful to an anonymous referee for helpful comments.
NR 73
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2013
VL 774
IS 2
AR 102
DI 10.1088/0004-637X/774/2/102
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211EW
UT WOS:000323888900011
ER
PT J
AU Aponte, JC
Elsila, JE
Burton, AS
Dworkin, JP
AF Aponte, Jose C.
Elsila, Jamie E.
Burton, Aaron S.
Dworkin, Jason P.
TI Chirality and compound-specific isotopic ratios of meteoritic aliphatic
amines
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Aponte, Jose C.; Elsila, Jamie E.; Burton, Aaron S.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Aponte, Jose C.; Elsila, Jamie E.; Burton, Aaron S.; Dworkin, Jason P.] Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Aponte, Jose C.] NASA, Postdoctoral Program, Oak Ridge, TN 37831 USA.
[Burton, Aaron S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM jose.c.aponte@nasa.gov
RI Burton, Aaron/H-2212-2011; Elsila, Jamie/C-9952-2012; Dworkin,
Jason/C-9417-2012
OI Burton, Aaron/0000-0002-7137-1605; Dworkin, Jason/0000-0002-3961-8997
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 584-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406361
ER
PT J
AU Baker, JS
Williams, TS
Miller, SG
Meador, MA
AF Baker, James S.
Williams, Tiffany S.
Miller, Sandi G.
Meador, Michael A.
TI Covalent crosslinking of carbon nanotube materials for improved tensile
strength
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Baker, James S.; Williams, Tiffany S.; Miller, Sandi G.; Meador, Michael A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM jsb39@zips.uakron.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 77-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406733
ER
PT J
AU Barrios, EA
Meador, MAB
Guo, HQ
Miranda, FA
Sandberg, A
Mcmillon, E
Nguyen, BN
Mueller, CH
AF Barrios, Elizabeth A.
Meador, Mary Ann B.
Guo, Haiquan
Miranda, Felix A.
Sandberg, Anna
Mcmillon, Emily
Nguyen, Baochau N.
Mueller, Carl H.
TI Fluorinated polyimide aerogels: Lightweight, low dielectric materials
for antenna substrates
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Barrios, Elizabeth A.] Wayne State Univ, Dept Chem Engn & Mat Sci, Detroit, MI 48193 USA.
[Barrios, Elizabeth A.; Meador, Mary Ann B.; Miranda, Felix A.; Sandberg, Anna; Mcmillon, Emily; Mueller, Carl H.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Guo, Haiquan; Nguyen, Baochau N.] Ohio Aerosp Inst, Cleveland, OH 44135 USA.
EM elizabeth.barrios.2013@gmail.com
NR 0
TC 0
Z9 0
U1 1
U2 5
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 240-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618407004
ER
PT J
AU Callahan, MP
Gerakines, PA
Martin, MG
Peeters, Z
Hudson, RL
AF Callahan, Michael P.
Gerakines, Perry A.
Martin, Mildred G.
Peeters, Zan
Hudson, Reggie L.
TI Irradiated benzene ice provides clues to meteoritic organic chemistry
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Callahan, Michael P.; Gerakines, Perry A.; Martin, Mildred G.; Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Martin, Mildred G.] Catholic Univ Amer, Washington, DC 20064 USA.
[Peeters, Zan] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
EM michael.p.callahan@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 528-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406312
ER
PT J
AU Cody, RJ
Smith, RL
AF Cody, Regina J.
Smith, Ramsey L.
TI Laboratory measurements of chemical reactions for atmospheres of the
Outer Planets and Titan
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Cody, Regina J.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
[Smith, Ramsey L.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA.
EM regina.cody@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 193-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406002
ER
PT J
AU Dworkin, JP
AF Dworkin, Jason P.
CA OSIRIS-REX Team
TI OSIRIS-REx will return a sample of asteroid 1999 RQ36 for astrochemistry
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Dworkin, Jason P.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM jason.p.dworkin@nasa.gov
RI Dworkin, Jason/C-9417-2012
OI Dworkin, Jason/0000-0002-3961-8997
NR 0
TC 0
Z9 0
U1 1
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 338-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406144
ER
PT J
AU Elsila, JE
Burton, AS
Callahan, MP
Dworkin, JP
Glavin, DP
AF Elsila, Jamie E.
Burton, Aaron S.
Callahan, Michael P.
Dworkin, Jason P.
Glavin, Daniel P.
TI Amino acids in carbonaceous chondrites and potential formation
mechanisms
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Elsila, Jamie E.; Burton, Aaron S.; Callahan, Michael P.; Dworkin, Jason P.; Glavin, Daniel P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
EM jamie.e.cook@nasa.gov
RI Burton, Aaron/H-2212-2011; Elsila, Jamie/C-9952-2012; Glavin,
Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012
OI Burton, Aaron/0000-0002-7137-1605; Glavin, Daniel/0000-0001-7779-7765;
Dworkin, Jason/0000-0002-3961-8997
NR 0
TC 0
Z9 0
U1 0
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 561-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406342
ER
PT J
AU Head-Gordon, M
Peverati, R
Bera, PP
Lee, TJ
AF Head-Gordon, Martin
Peverati, Roberto
Bera, Partha P.
Lee, Timothy J.
TI Electronic structure calculations for understanding the association and
growth of small carbon clusters
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Head-Gordon, Martin; Peverati, Roberto] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
[Bera, Partha P.; Lee, Timothy J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
EM mhg@cchem.berkeley.edu
NR 0
TC 0
Z9 0
U1 1
U2 2
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 229-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406035
ER
PT J
AU Hudson, RL
Gerakines, PA
Loeffler, MJ
Moore, MH
Ferrante, RF
AF Hudson, Reggie L.
Gerakines, Perry A.
Loeffler, Mark J.
Moore, Marla H.
Ferrante, Robert F.
TI Molecules and molecular evolution in cold extraterrestrial environments:
The chemist's approach
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Hudson, Reggie L.; Gerakines, Perry A.; Loeffler, Mark J.; Moore, Marla H.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ferrante, Robert F.] US Naval Acad, Dept Chem, Annapolis, MD 21402 USA.
EM reggie.hudson@nasa.gov
RI Loeffler, Mark/C-9477-2012
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 337-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406143
ER
PT J
AU Hudson, RL
AF Hudson, Reggie L.
TI Samuel C. Lind: Father of US radiation chemistry
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
EM reggie.hudson@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 4-HIST
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618403860
ER
PT J
AU Langhoff, PW
Ben-Nun, M
Rollin, K
Mills, JD
Boatz, JA
Hinde, RJ
Sheehy, JA
Gallup, GA
AF Langhoff, Peter W.
Ben-Nun, Michal
Rollin, Kyle
Mills, Jeffrey D.
Boatz, Jerry A.
Hinde, Robert J.
Sheehy, Jeffrey A.
Gallup, Gordon A.
TI Exact atomic-pair-based ab initio calculations of molecular potential
energy surfaces
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Langhoff, Peter W.; Ben-Nun, Michal; Rollin, Kyle] Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA.
[Mills, Jeffrey D.; Boatz, Jerry A.] Air Force Res Lab, RQRP, Edwards AFB, CA 93524 USA.
[Hinde, Robert J.] Univ Tennessee, Dept Chem, Knoxville, TN 37996 USA.
[Sheehy, Jeffrey A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Gallup, Gordon A.] Univ Nebraska, Dept Phys & Astron, Lincoln, NE 68588 USA.
EM planghoff@ucsd.edu
NR 0
TC 0
Z9 0
U1 0
U2 2
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 191-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618402715
ER
PT J
AU Lin, Y
Kim, JW
Funk, MR
Connell, JW
AF Lin, Yi
Kim, Jae-Woo
Funk, Michael R.
Connell, John W.
TI Holey graphenes as lightweight platforms toward composite and energy
storage applications
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Lin, Yi; Kim, Jae-Woo] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Funk, Michael R.] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA.
[Connell, John W.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA.
EM yi.lin@nianet.org
RI Kim, Jae-Woo/A-8314-2008
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 223-ENFL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618403182
ER
PT J
AU Mathies, RA
Kaiser, RI
Stockton, A
Kim, YS
Jensen, E
AF Mathies, Richard A.
Kaiser, Ralf I.
Stockton, Amanda
Kim, Yong S.
Jensen, Erik
TI On the use of microfluidic chemical and biochemical analysis devices to
detect dipeptides synthesized in interstellar model ices
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Mathies, Richard A.; Jensen, Erik] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
[Kaiser, Ralf I.; Kim, Yong S.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
[Stockton, Amanda] CALTECH, Jet Prop Lab, Pasadena, CA 01109 USA.
EM ramathies@berkeley.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 558-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406339
ER
PT J
AU Meador, MAB
Guo, HQ
Mesick, NJ
AF Meador, Mary Ann B.
Guo, Haiquan
Mesick, Nathaniel J.
TI Polyimide aerogels for use as insulation for flexible thermal protection
systems for inflatable aerodynamic decelerators
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Meador, Mary Ann B.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Guo, Haiquan] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Mesick, Nathaniel J.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
EM maryann.meador@nasa.gov
NR 0
TC 0
Z9 1
U1 1
U2 6
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 138-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406793
ER
PT J
AU Meador, MA
AF Meador, Michael A.
TI Development of lightweight composites from carbon nanotube
reinforcements
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Meador, Michael A.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
EM Michael.A.Meador@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 73-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406729
ER
PT J
AU Pettit, D
AF Pettit, Donald
TI On the frontier: Some observations of surface tension phenomena from the
International Space Station
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Pettit, Donald] NASA JSC, CB, Houston, TX 77058 USA.
EM donald.r.pettit@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 384-COLL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618402401
ER
PT J
AU Silva, R
Hodyss, R
Johnson, PV
AF Silva, Rebecca
Hodyss, Robert
Johnson, Paul V.
TI UV stimulated fluorescence studies of PAH-water ice mixtures
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Silva, Rebecca] Univ Texas Brownsville, Dept Chem & Environm Sci, Brownsville, TX 78520 USA.
[Hodyss, Robert; Johnson, Paul V.] CALTECH, Jet Prop Lab, Planetary Ices Grp, Pasadena, CA 91109 USA.
EM beckas225@sbcglobal.net
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 194-PHYS
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406003
ER
PT J
AU Williams, JC
Meador, MAB
AF Williams, Jarrod C.
Meador, Mary Ann B.
TI Synthesis and characterization of a new family of polyamide aerogels by
cross-linking amine capped polyamide oligomers
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Williams, Jarrod C.; Meador, Mary Ann B.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
EM jarrod.c.williams@nasa.gov
NR 0
TC 0
Z9 0
U1 1
U2 4
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 140-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618406795
ER
PT J
AU Wohl, CJ
Palmieri, FL
Lin, Y
Jackson, AM
Cisotto, AA
Sheplak, M
Connell, JW
AF Wohl, Christopher J.
Palmieri, Frank L.
Lin, Yi
Jackson, Allen M.
Cisotto, Alexxandra A.
Sheplak, Mark
Connell, John W.
TI Shear stress sensing using elastomer micropillar arrays
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 246th National Meeting of the American-Chemical-Society (ACS)
CY SEP 08-12, 2013
CL Indianapolis, IN
SP Amer Chem Soc
C1 [Wohl, Christopher J.; Palmieri, Frank L.; Jackson, Allen M.; Connell, John W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
[Lin, Yi] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Cisotto, Alexxandra A.] NASA, LaRC Undergrad Student Res Program, Hampton, VA 23681 USA.
[Sheplak, Mark] Univ Florida, Gainesville, FL 32605 USA.
EM christopher.j.wohl@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD SEP 8
PY 2013
VL 246
MA 282-POLY
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 288NJ
UT WOS:000329618407044
ER
PT J
AU Frisch, PC
Bzowski, M
Livadiotis, G
McComas, DJ
Moebius, E
Mueller, HR
Pryor, WR
Schwadron, NA
Sokol, JM
Vallerga, JV
Ajello, JM
AF Frisch, P. C.
Bzowski, M.
Livadiotis, G.
McComas, D. J.
Moebius, E.
Mueller, H. -R.
Pryor, W. R.
Schwadron, N. A.
Sokol, J. M.
Vallerga, J. V.
Ajello, J. M.
TI Decades-Long Changes of the Interstellar Wind Through Our Solar System
SO SCIENCE
LA English
DT Article
ID PICKUP IONS; HELIUM; PARAMETERS; MARINER-10; IBEX; GAS
AB The journey of the Sun through the dynamically active local interstellar medium creates an evolving heliosphere environment. This motion drives a wind of interstellar material through the heliosphere that has been measured with Earth-orbiting and interplanetary spacecraft for 40 years. Recent results obtained by NASA's Interstellar Boundary Explorer mission during 2009-2010 suggest that neutral interstellar atoms flow into the solar system from a different direction than found previously. These prior measurements represent data collected from Ulysses and other spacecraft during 1992-2002 and a variety of older measurements acquired during 1972-1978. Consideration of all data types and their published results and uncertainties, over the three epochs of observations, indicates that the trend for the interstellar flow ecliptic longitude to increase linearly with time is statistically significant.
C1 [Frisch, P. C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Bzowski, M.; Sokol, J. M.] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland.
[Livadiotis, G.; McComas, D. J.] SW Res Inst, San Antonio, TX 78249 USA.
[McComas, D. J.] Univ Texas San Antonio, San Antonio, TX 78249 USA.
[Moebius, E.; Schwadron, N. A.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Mueller, H. -R.] Dartmouth Coll, Hanover, NH 03755 USA.
[Pryor, W. R.] Cent Arizona Coll, Coolidge, AZ 85128 USA.
[Vallerga, J. V.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Ajello, J. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Frisch, PC (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM frisch@oddjob.uchicago.edu
RI Sokol, Justyna/K-2892-2015;
OI Mueller, Hans-Reinhard/0000-0001-7364-5377; Moebius,
Eberhard/0000-0002-2745-6978
FU NASA Explorers Program; Polish Ministry of Science and Higher Education
[N-N203-513-038]; NASA [NNX10AC44G]
FX We thank everyone who made the IBEX mission a reality. IBEX is primarily
funded by the NASA Explorers Program. Polish contributions were
supported by a Polish Ministry of Science and Higher Education grant,
N-N203-513-038. Additional support was provided by NASA grant
NNX10AC44G. We thank R. R. Meier for many helpful comments and D. E.
Welty for his reductions of the Sirius Ca+ data. IBEX data
have been archived and are available from the IBEX project and the NASA
National Space Science Data Center.
NR 19
TC 34
Z9 34
U1 0
U2 14
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD SEP 6
PY 2013
VL 341
IS 6150
BP 1080
EP 1082
DI 10.1126/science.1239925
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 211TG
UT WOS:000323933100035
PM 24009386
ER
PT J
AU Graven, HD
Keeling, RF
Piper, SC
Patra, PK
Stephens, BB
Wofsy, SC
Welp, LR
Sweeney, C
Tans, PP
Kelley, JJ
Daube, BC
Kort, EA
Santoni, GW
Bent, JD
AF Graven, H. D.
Keeling, R. F.
Piper, S. C.
Patra, P. K.
Stephens, B. B.
Wofsy, S. C.
Welp, L. R.
Sweeney, C.
Tans, P. P.
Kelley, J. J.
Daube, B. C.
Kort, E. A.
Santoni, G. W.
Bent, J. D.
TI Enhanced Seasonal Exchange of CO2 by Northern Ecosystems Since 1960
SO SCIENCE
LA English
DT Article
ID ATMOSPHERIC CARBON-DIOXIDE; AMPLITUDE INCREASE; PLANT-GROWTH; MAUNA-LOA;
VEGETATION; CLIMATE; TRENDS; ALASKA; DISTURBANCE; FORESTS
AB Seasonal variations of atmospheric carbon dioxide (CO2) in the Northern Hemisphere have increased since the 1950s, but sparse observations have prevented a clear assessment of the patterns of long-term change and the underlying mechanisms. We compare recent aircraft-based observations of CO2 above the North Pacific and Arctic Oceans to earlier data from 1958 to 1961 and find that the seasonal amplitude at altitudes of 3 to 6 km increased by 50% for 45 degrees to 90 degrees N but by less than 25% for 10 degrees to 45 degrees N. An increase of 30 to 60% in the seasonal exchange of CO2 by northern extratropical land ecosystems, focused on boreal forests, is implicated, substantially more than simulated by current land ecosystem models. The observations appear to signal large ecological changes in northern forests and a major shift in the global carbon cycle.
C1 [Graven, H. D.; Keeling, R. F.; Piper, S. C.; Welp, L. R.; Bent, J. D.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Patra, P. K.] Res Inst Global Change, Yokohama, Kanagawa, Japan.
[Stephens, B. B.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Wofsy, S. C.; Daube, B. C.; Santoni, G. W.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Sweeney, C.; Tans, P. P.] NOAA, Boulder, CO USA.
[Kelley, J. J.] Univ Alaska, Inst Marine Sci, Fairbanks, AK 99775 USA.
[Kort, E. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Graven, HD (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
EM hgraven@ucsd.edu
RI Kort, Eric/F-9942-2012; Stephens, Britton/B-7962-2008;
OI Kort, Eric/0000-0003-4940-7541; Stephens, Britton/0000-0002-1966-6182;
Graven, Heather/0000-0003-3934-2502
FU DOE [DE-SC0005090]; NSF [ATM-0628575, ATM-0628519, ATM-0628388,
ATM-0628452, ATM-1036399]; National Center for Atmospheric Research
(NCAR); NASA [NNX11AF36G]; U.S. Navy/Office of Naval Research
[N00014-67-A-0103-0007]; NSF; Ministry of Education, Culture, Sports,
Science and Technology Green Network of Excellence program;
Environmental Protection Agency's Science to Achieve Results program
FX The Scripps CO2 Program is supported by DOE grant
DE-SC0005090. HIPPO was supported by NSF grants ATM-0628575,
ATM-0628519, ATM-0628388, ATM-0628452, and ATM-1036399, and by the
National Center for Atmospheric Research (NCAR). Recovery and updating
of early aircraft, MLO, and BRW data was supported by NSF grant
ATM-1036399. L. R. W. was supported by NASA award NNX11AF36G. Early
observations at BRW were funded by U.S. Navy/Office of Naval Research
contract N00014-67-A-0103-0007. Online access to all observational data
is summarized in section SM10 of the supplementary materials. NCAR is
supported by the NSF. Any opinions, findings, and conclusions or
recommendations expressed in this material are those of the authors and
do not necessarily reflect the views of NOAA, NSF, DOE or NASA. We thank
the HIPPO science team and the crew and support staff at the NCAR
Research Aviation Facility. We acknowledge the World Climate Research
Programme's Working Group on Coupled Modelling, which is responsible for
CMIP, and we thank the climate modeling groups for producing and making
available their model output. Support of the CMIP data sets is provided
by the Office of Science, U.S. Department of Energy. C. Roedenbeck
provided assistance with the TM3 model. P. K. P. is partially supported
by the Ministry of Education, Culture, Sports, Science and Technology
Green Network of Excellence program. G. W. S. acknowledges support from
the NSF Graduate Research Fellowship Program and the Environmental
Protection Agency's Science to Achieve Results program.
NR 44
TC 77
Z9 77
U1 13
U2 190
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD SEP 6
PY 2013
VL 341
IS 6150
BP 1085
EP 1089
DI 10.1126/science.1239207
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 211TG
UT WOS:000323933100037
PM 23929948
ER
PT J
AU Freissinet, C
Buch, A
Szopa, C
Sternberg, R
AF Freissinet, C.
Buch, A.
Szopa, C.
Sternberg, R.
TI Enantiomeric separation of volatile organics by gas chromatography for
the in situ analysis of extraterrestrial materials: Kinetics and
thermodynamics investigation of various chiral stationary phases
SO JOURNAL OF CHROMATOGRAPHY A
LA English
DT Article
DE Chirality; Space analysis; Volatile organics
ID PERMETHYLATED BETA-CYCLODEXTRIN; MURCHISON METEORITE; AMINO-ACIDS;
GAMMA-CYCLODEXTRIN; MARS; ENANTIOSELECTIVITY; ASSOCIATION; DERIVATIVES;
MECHANISMS; RESOLUTION
AB The performances of several commercial chiral capillary columns have been evaluated with the aim of determining the one most suitable for enantiomeric separation in a gas chromatograph onboard a space probe. We compared the GC MS response of three capillary columns coated with different chiral stationary phases (CSP) using volatile chiral organic molecules which are potential markers of a prebiotic organic chemistry. The three different chiral capillary columns are Chirasil-Val, with an amino acid derivative CSP, ChiralDex-beta-PM, with a CSP composed of dissolved permethylated beta-cyclodextrins in polysiloxane, and Chirasil-Dex, with a CSP made of modified cyclodextrins chemically bonded to the polysiloxane backbone. Both kinetics and thermodynamics studies have been carried out to evaluate the chiral recognition potential in these different types of columns. The thermodynamic parameters also allow a better understanding of the driving forces affecting the retention and separation of the enantiomers. The Chirasil-Dex-CSP displays the best characteristics for an optimal resolution of the chiral compounds, without preliminary derivatization. This CSP had been chosen to be the only chiral column in the Sample Analysis at Mars (SAM) experiment onboard the current Mars Science Laboratory (MSL) mission, and is also part of the Mars Organic Molecules Analyzer (MOMA) gas chromatograph onboard the next Martian mission ExoMars. The use of this column could also be extended to all space missions aimed at studying chirality in space. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Freissinet, C.; Buch, A.] Ecole Cent Paris, Lab Genie Precedes & Mat LGPM, F-92295 Chatenay Malabry, France.
[Freissinet, C.; Sternberg, R.] Univ Paris 07, Univ Paris Est Creteil, LISA, F-94010 Creteil, France.
[Freissinet, C.; Sternberg, R.] CNRS, UMR 7583, F-94010 Creteil, France.
[Szopa, C.] Univ Versailles St Quentin, Lab Atmospheres Milieux Observat Spatiales LATMOS, Univ Paris 06, F-75005 Paris, France.
[Szopa, C.] CNRS, F-75005 Paris, France.
RP Freissinet, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM caroline.freissinet@nasa.gov
RI szopa, cyril/C-6865-2015
OI szopa, cyril/0000-0002-0090-4056
NR 44
TC 7
Z9 7
U1 2
U2 58
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0021-9673
J9 J CHROMATOGR A
JI J. Chromatogr. A
PD SEP 6
PY 2013
VL 1306
BP 59
EP 71
DI 10.1016/j.chroma.2013.07.058
PG 13
WC Biochemical Research Methods; Chemistry, Analytical
SC Biochemistry & Molecular Biology; Chemistry
GA 207IA
UT WOS:000323590900007
PM 23921265
ER
PT J
AU Asefi-Najafabady, S
Saatchi, S
AF Asefi-Najafabady, Salvi
Saatchi, Sassan
TI Response of African humid tropical forests to recent rainfall anomalies
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE African rainforest; drought; climate change; resilience
ID AMAZON FOREST; 2005 DROUGHT; WEST-AFRICA; EL-NINO; CLIMATE; MORTALITY;
SEASONALITY; TRENDS
AB During the last decade, strong negative rainfall anomalies resulting from increased sea surface temperature in the tropical Atlantic have caused extensive droughts in rainforests of western Amazonia, exerting persistent effects on the forest canopy. In contrast, there have been no significant impacts on rainforests of West and Central Africa during the same period, despite large-scale droughts and rainfall anomalies during the same period. Using a combination of rainfall observations from meteorological stations from the Climate Research Unit (CRU; 1950-2009) and satellite observations of the Tropical Rainfall Measuring Mission (TRMM; 1998-2010), we show that West and Central Africa experienced strong negative water deficit (WD) anomalies over the last decade, particularly in 2005, 2006 and 2007. These anomalies were a continuation of an increasing drying trend in the region that started in the 1970s. We monitored the response of forests to extreme rainfall anomalies of the past decade by analysing the microwave scatterometer data from QuickSCAT (1999-2009) sensitive to variations in canopy water content and structure. Unlike in Amazonia, we found no significant impacts of extreme WD events on forests of Central Africa, suggesting potential adaptability of these forests to short-term severe droughts. Only forests near the savanna boundary in West Africa and in fragmented landscapes of the northern Congo Basin responded to extreme droughts with widespread canopy disturbance that lasted only during the period of WD. Time-series analyses of CRU and TRMM data show most regions in Central and West Africa experience seasonal or decadal extreme WDs (less than 2600 mm). We hypothesize that the long-term historical extreme WDs with gradual drying trends in the 1970s have increased the adaptability of humid tropical forests in Africa to droughts.
C1 [Asefi-Najafabady, Salvi; Saatchi, Sassan] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA 90095 USA.
[Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Asefi-Najafabady, S (reprint author), Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA 90095 USA.
EM salvi.asefi@asu.edu
FU NASA grants at the Jet Propulsion Laboratory
FX The research was partially supported by NASA grants at the Jet
Propulsion Laboratory.
NR 42
TC 19
Z9 19
U1 7
U2 34
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8436
EI 1471-2970
J9 PHILOS T R SOC B
JI Philos. Trans. R. Soc. B-Biol. Sci.
PD SEP 5
PY 2013
VL 368
IS 1625
AR 20120306
DI 10.1098/rstb.2012.0306
PG 8
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA AA6PO
UT WOS:000331220500010
PM 23878335
ER
PT J
AU Fisher, JB
Sikka, M
Sitch, S
Ciais, P
Poulter, B
Galbraith, D
Lee, JE
Huntingford, C
Viovy, N
Zeng, N
Ahlstrom, A
Lomas, MR
Levy, PE
Frankenberg, C
Saatchi, S
Malhi, Y
AF Fisher, Joshua B.
Sikka, Munish
Sitch, Stephen
Ciais, Philippe
Poulter, Benjamin
Galbraith, David
Lee, Jung-Eun
Huntingford, Chris
Viovy, Nicolas
Zeng, Ning
Ahlstrom, Anders
Lomas, Mark R.
Levy, Peter E.
Frankenberg, Christian
Saatchi, Sassan
Malhi, Yadvinder
TI African tropical rainforest net carbon dioxide fluxes in the twentieth
century
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE Africa; carbon; Congo; rainforest; tropic; uncertainty
ID GLOBAL VEGETATION MODELS; SPACE-TIME CLIMATE; ATMOSPHERIC CO2; ELEVATED
CO2; LAND-USE; TERRESTRIAL ECOSYSTEM; SURFACE CLIMATE; RECENT TRENDS;
DROUGHT; BALANCE
AB The African humid tropical biome constitutes the second largest rainforest region, significantly impacts global carbon cycling and climate, and has undergone major changes in functioning owing to climate and land-use change over the past century. We assess changes and trends in CO2 fluxes from 1901 to 2010 using nine land surface models forced with common driving data, and depict the inter-model variability as the uncertainty in fluxes. The biome is estimated to be a natural (no disturbance) net carbon sink (-0.02 kg C m(-2) yr(-1) or -0.04 Pg C yr(-1), p < 0.05) with increasing strength fourfold in the second half of the century. The models were in close agreement on net CO2 flux at the beginning of the century (sigma 1901 = 0.02 kg C m(-2) yr(-1)), but diverged exponentially throughout the century (sigma 2010 = 0.03 kg C m(-2) yr(-1)). The increasing uncertainty is due to differences in sensitivity to increasing atmospheric CO2, but not increasing water stress, despite a decrease in precipitation and increase in air temperature. However, the largest uncertainties were associated with the most extreme drought events of the century. These results highlight the need to constrain modelled CO2 fluxes with increasing atmospheric CO2 concentrations and extreme climatic events, as the uncertainties will only amplify in the next century.
C1 [Fisher, Joshua B.; Sikka, Munish; Lee, Jung-Eun; Frankenberg, Christian; Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sitch, Stephen] Univ Exeter, Coll Life & Environm Sci, Dept Geog, Exeter EX4 4RJ, Devon, England.
[Ciais, Philippe; Poulter, Benjamin; Viovy, Nicolas] Orme Merisiers, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France.
[Galbraith, David] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
[Huntingford, Chris] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England.
[Zeng, Ning] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Ahlstrom, Anders] Lund Univ, Dept Phys Geog & Ecosyst Sci, S-22362 Lund, Sweden.
[Lomas, Mark R.] Univ Sheffield, Dept Anim & Plant Sci, Ctr Terr Carbon Dynam, Sheffield S10 2TN, S Yorkshire, England.
[Levy, Peter E.] Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland.
[Malhi, Yadvinder] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford OX1 3QY, England.
RP Fisher, JB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jbfisher@jpl.nasa.gov
RI Huntingford, Chris/A-4307-2008; Zeng, Ning/A-3130-2008; Sitch,
Stephen/F-8034-2015; Frankenberg, Christian/A-2944-2013; Ahlstrom,
Anders/F-3215-2017;
OI Zeng, Ning/0000-0002-7489-7629; Sitch, Stephen/0000-0003-1821-8561;
Frankenberg, Christian/0000-0002-0546-5857; Ahlstrom,
Anders/0000-0003-1642-0037; Huntingford, Chris/0000-0002-5941-7770;
Fisher, Joshua/0000-0003-4734-9085; Poulter,
Benjamin/0000-0002-9493-8600
FU California Institute of Technology. Government
FX The research described in this paper was performed by the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. We thank S. Levis and
S. Zaehle, who contributed model output for CLM4-CN and OCN,
respectively, and J.-H. Lee for GIS input. Copyright 2013 California
Institute of Technology. Government sponsorship acknowledged. J.B.F. and
S.S. formulated idea; J.B.F. designed research; M.S. and J.B.F.
performed research; all authors contributed to the writing of the paper.
The authors declare no conflict of interest.
NR 78
TC 15
Z9 15
U1 4
U2 41
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8436
EI 1471-2970
J9 PHILOS T R SOC B
JI Philos. Trans. R. Soc. B-Biol. Sci.
PD SEP 5
PY 2013
VL 368
IS 1625
AR 20120376
DI 10.1098/rstb.2012.0376
PG 9
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA AA6PO
UT WOS:000331220500015
PM 23878340
ER
PT J
AU Rudolph, JK
Bernitt, S
Epp, SW
Steinbrugge, R
Beilmann, C
Brown, GV
Eberle, S
Graf, A
Harman, Z
Hell, N
Leutenegger, M
Muller, A
Schlage, K
Wille, HC
Yavas, H
Ullrich, J
Lopez-Urrutia, JRC
AF Rudolph, J. K.
Bernitt, S.
Epp, S. W.
Steinbruegge, R.
Beilmann, C.
Brown, G. V.
Eberle, S.
Graf, A.
Harman, Z.
Hell, N.
Leutenegger, M.
Mueller, A.
Schlage, K.
Wille, H. -C.
Yavas, H.
Ullrich, J.
Lopez-Urrutia, J. R. Crespo
TI X-Ray Resonant Photoexcitation: Linewidths and Energies of K alpha
Transitions in Highly Charged Fe Ions
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID HIGH-RESOLUTION MEASUREMENTS; ACTIVE GALACTIC NUCLEI; HELIUM-LIKE IONS;
ACCRETION DISK; EMISSION-LINES; IRON; SPECTRA; DIAGNOSTICS; RATES; XXV
AB Photoabsorption by and fluorescence of the K alpha transitions in highly charged iron ions are essential mechanisms for x-ray radiation transfer in astrophysical environments. We study photoabsorption due to the main K alpha transitions in highly charged iron ions from heliumlike to fluorinelike (Fe24+ to Fe17+) using monochromatic x rays around 6.6 keV at the PETRA III synchrotron photon source. Natural linewidths were determined with hitherto unattained accuracy. The observed transitions are of particular interest for the understanding of photoexcited plasmas found in x-ray binary stars and active galactic nuclei.
C1 [Rudolph, J. K.; Bernitt, S.; Steinbruegge, R.; Beilmann, C.; Eberle, S.; Harman, Z.; Ullrich, J.; Lopez-Urrutia, J. R. Crespo] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Rudolph, J. K.; Mueller, A.] Univ Giessen, Inst Atom & Mol Phys, D-35392 Giessen, Germany.
[Epp, S. W.] CFEL, Max Planck Adv Study Grp, D-22607 Hamburg, Germany.
[Beilmann, C.] Heidelberg Univ, Inst Phys, D-69120 Heidelberg, Germany.
[Brown, G. V.; Graf, A.; Hell, N.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Harman, Z.] ExtreMe Matter Inst EMMI, D-64291 Darmstadt, Germany.
[Hell, N.] Univ Erlangen Nurnberg, Dr Karl Remeis Observ, D-96049 Bamberg, Germany.
[Hell, N.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany.
[Leutenegger, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Leutenegger, M.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Schlage, K.; Wille, H. -C.; Yavas, H.] Deutsch Elektronen Synchrotron PETRA III, D-22607 Hamburg, Germany.
RP Rudolph, JK (reprint author), Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany.
EM jan.rudolph@mpi-hd.mpg.de
RI Yavas, Hasan/A-7164-2014; Muller, Alfred/A-3548-2009; Wille,
Hans-Christian/C-3881-2013; Crespo Lopez-Urrutia, Jose R./F-7069-2011;
OI Yavas, Hasan/0000-0002-8940-3556; Muller, Alfred/0000-0002-0030-6929;
Crespo Lopez-Urrutia, Jose R./0000-0002-2937-8037; Hell,
Natalie/0000-0003-3057-1536
FU Deutsche Forschungsgemeinschaft (DFG); DESY, a member of the Helmholtz
Association (HGF); U.S. Department of Energy [DE-AC52-07NA27344]; NASA;
Bundesministerium fur Wirtschaft und Technologie (BMWi) under Deutsches
Zentrum fur Luft- und Raumfahrt (DLR) [50 OR 1113]; EMMI
FX The research leading to these results was supported by Deutsche
Forschungsgemeinschaft (DFG). J. K. R., N. H., and C. B. received
funding from DESY, a member of the Helmholtz Association (HGF). Work by
LLNL was performed under the auspices of the U.S. Department of Energy
under Contract No. DE-AC52-07NA27344 and supported by NASA grants. N. H.
also received funding from Bundesministerium fur Wirtschaft und
Technologie (BMWi) under Deutsches Zentrum fur Luft- und Raumfahrt (DLR)
Grant No. 50 OR 1113. Z.H.'s work was supported by EMMI.
NR 53
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U1 0
U2 15
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD SEP 5
PY 2013
VL 111
IS 10
AR 103002
DI 10.1103/PhysRevLett.111.103002
PG 6
WC Physics, Multidisciplinary
SC Physics
GA 215TE
UT WOS:000324232600011
PM 25166661
ER
PT J
AU Aasi, J
Abadie, J
Abbott, BP
Abbott, R
Abbott, TD
Abernathy, M
Accadia, T
Acernese, F
Adams, C
Adams, T
Addesso, P
Adhikari, R
Affeldt, C
Agathos, M
Agatsuma, K
Ajith, P
Allen, B
Allocca, A
Ceron, EA
Amariutei, D
Anderson, SB
Anderson, WG
Arai, K
Araya, MC
Ast, S
Aston, SM
Astone, P
Atkinson, D
Aufmuth, P
Aulbert, C
Aylott, BE
Babak, S
Baker, P
Ballardin, G
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CA LIGO-Virgo Sci Collaboration
TI Parameter estimation for compact binary coalescence signals with the
first generation gravitational-wave detector network
SO PHYSICAL REVIEW D
LA English
DT Article
ID ELECTROMAGNETIC COUNTERPARTS; MASS-DISTRIBUTION; BLACK-HOLES;
TRANSIENTS; INSPIRALS; COSMOLOGY; PHYSICS; SEARCH
AB Compact binary systems with neutron stars or black holes are one of the most promising sources for ground-based gravitational-wave detectors. Gravitational radiation encodes rich information about source physics; thus parameter estimation and model selection are crucial analysis steps for any detection candidate events. Detailed models of the anticipated waveforms enable inference on several parameters, such as component masses, spins, sky location and distance, that are essential for new astrophysical studies of these sources. However, accurate measurements of these parameters and discrimination of models describing the underlying physics are complicated by artifacts in the data, uncertainties in the waveform models and in the calibration of the detectors. Here we report such measurements on a selection of simulated signals added either in hardware or software to the data collected by the two LIGO instruments and the Virgo detector during their most recent joint science run, including a "blind injection'' where the signal was not initially revealed to the collaboration. We exemplify the ability to extract information about the source physics on signals that cover the neutron-star and black-hole binary parameter space over the component mass range 1M(circle dot)-25M(circle dot) and the full range of spin parameters. The cases reported in this study provide a snapshot of the status of parameter estimation in preparation for the operation of advanced detectors.
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[Abbott, T. D.; Griffo, C.; Smith, J. R.] Calif State Univ Fullerton, Fullerton, CA 92831 USA.
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[Accadia, T.; Bebronne, M.; Buskulic, D.; Dietz, A.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Tournefier, E.; Verkindt, D.; Yvert, M.] Univ Savoie, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France.
[Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Forte, L. A.; Garufi, F.; Milano, L.; Mosca, S.; Parisi, M.; Persichetti, G.; Romano, R.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy.
[Calloni, E.; De Rosa, R.; Garufi, F.; Milano, L.; Mosca, S.; Parisi, M.; Persichetti, G.] Univ Naples Federico II, I-80126 Naples, Italy.
[Acernese, F.; Barone, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy.
[Adams, C.; Aston, S. M.; Betzwieser, J.; Birch, J.; Bridges, D. O.; Cowart, M.; Evans, T.; Forsi, E.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Guido, C.; Hanson, J.; Heintze, M. C.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Kinzel, D. L.; Le Roux, A.; Lormand, M.; Meyer, M. S.; Nolting, D.; O'Reilly, B.; Overmier, H.; Ramet, C.; Riesen, R.; Roddy, S.; Romie, J. H.; Sellers, D.; Stuver, A. L.; Thorne, K. A.; Traylor, G.; Welborn, T.; Wooley, R.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA.
[Adams, T.; Dent, T.; Edwards, M.; Fairhurst, S.; Macleod, D. M.; Messenger, C.; Nuttall, L.; Predoi, V.; Robinson, C.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Veitch, J.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Pierro, V.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[Affeldt, C.; Allen, B.; Ast, S.; Aufmuth, P.; Aulbert, C.; Bauchrowitz, J.; Bertolini, A.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Damjanic, M.; Danzmann, K.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Heurs, M.; Hewitson, M.; Kaufer, H.; Kawazoe, F.; Keitel, D.; Khalaidovski, A.; Kim, H.; Kringel, V.; Kuehn, G.; Lastzka, N.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mossavi, K.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Puncken, O.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schulz, B.; Shaltev, M.; Simakov, D.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Thuering, A.; Vahlbruch, H.; Wanner, A.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Wiesner, K.; Willke, B.; Wimmer, M.; Winkelmann, L.; Winkler, W.; Wittel, H.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Affeldt, C.; Allen, B.; Ast, S.; Aufmuth, P.; Aulbert, C.; Bauchrowitz, J.; Bertolini, A.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Damjanic, M.; Danzmann, K.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Heurs, M.; Hewitson, M.; Kaufer, H.; Kawazoe, F.; Keitel, D.; Khalaidovski, A.; Kim, H.; Kringel, V.; Kuehn, G.; Lastzka, N.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mossavi, K.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Puncken, O.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schulz, B.; Shaltev, M.; Simakov, D.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Thuering, A.; Wanner, A.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Wiesner, K.; Willke, B.; Wimmer, M.; Winkelmann, L.; Winkler, W.; Wittel, H.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Agathos, M.; Bauer, Th. S.; Beker, M. G.; Blom, M.; Bulten, H. J.; Del Pozzo, W.; Jonker, R. J. G.; Li, T. G. F.; Rabeling, D. S.; ter Braack, A. P. M.; van den Brand, J. F. J.; Van Den Broeck, C.; van der Putten, S.; Veitch, J.; Vitale, S.] Nikhef, NL-1098 XG Amsterdam, Netherlands.
[Bulten, H. J.; Rabeling, D. S.; van den Brand, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands.
[Agatsuma, K.; Fujimoto, M. -K.; Hayama, K.; Izumi, K.; Kawamura, S.; Mori, T.; Nishizawa, A.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Allen, B.; Ceron, E. Amador; Anderson, W. G.; Brady, P. R.; Clayton, J. H.; Creighton, J. D. E.; Favata, M.; Giampanis, S.; Hammer, D.; Hughey, B.; Kline, J.; Koranda, S.; Mercer, R. A.; Moe, B.; Ochsner, E.; Oldenberg, R. G.; O'Shaughnessy, R.; Pankow, C.; Papa, M. A.; Siemens, X.; Skelton, G. R.; Wade, L.; Wade, M.; Wiseman, A. G.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Allocca, A.; Basti, A.; Bitossi, M.; Bonelli, L.; Boschi, V.; Braccini, S.; Bradaschia, C.; Cella, G.; Colacino, C. N.; Di Lieto, A.; Di Virgilio, A.; Ferrante, I.; Fidecaro, F.; Frasconi, F.; Gennai, A.; Giazotto, A.; Mantovani, M.; Paoletti, F.; Paoletti, R.; Passaquieti, R.; Passuello, D.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Torre, O.; Vajente, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Basti, A.; Bonelli, L.; Colacino, C. N.; Di Lieto, A.; Ferrante, I.; Fidecaro, F.; Passaquieti, R.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Vajente, G.] Univ Pisa, I-56127 Pisa, Italy.
[Allocca, A.; Paoletti, R.; Torre, O.] Univ Siena, I-53100 Siena, Italy.
[Amariutei, D.; Bao, Y.; Ciani, G.; Feldbaum, D.; Gleason, J.; Hartman, M. T.; Klimenko, S.; Liu, Z.; Martin, R. M.; Mitselmakher, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Necula, V.; Ottens, R. S.; Tanner, D. B.; Whiting, B. F.; Williams, L.] Univ Florida, Gainesville, FL 32611 USA.
[Astone, P.; Colla, A.; Conte, A.; Frasca, S.; Majorana, E.; Naticchioni, L.; Palomba, C.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
[Colla, A.; Colombini, M.; Conte, A.; Frasca, S.; Naticchioni, L.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Atkinson, D.; Barker, D.; Barton, M. A.; Batch, J.; Berliner, J. M.; Bland, B.; Clara, F.; Cook, D.; Garcia, J.; Gray, C.; Hanks, J.; Ingram, D. R.; Kawabe, K.; Landry, M.; Lhuillier, V.; Lubinski, M.; McCarthy, R.; Mendell, G.; Moraru, D.; Moreno, G.; Raab, F. J.; Radkins, H.; Reed, C. M.; Rodruck, M.; Ryan, K.; Sandberg, V.; Savage, R. L.; Schwinberg, P.; Sigg, D.; Steinert, E.; Thomas, P.; Vorvick, C.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA.
[Aylott, B. E.; Bond, C.; Carbone, L.; Cruise, A. M.; Cutler, R. M.; Freise, A.; Fulda, P. J.; Grover, K.; Hallam, J. M.; Haster, C. -J.; Lodhia, D.; Mandel, I.; Mingarelli, C. M. F.; Page, A.; Sidery, T. L.; Smith, R. J. E.; Vecchio, A.; Wang, M.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Babak, S.; Behnke, B.; Grunewald, S.; Krishnan, B.; Leaci, P.; Papa, M. A.; Robinson, E. L.; Schutz, B. F.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Baker, P.; Cornish, N.] Montana State Univ, Bozeman, MT 59717 USA.
[Ballardin, G.; Canuel, B.; Carbognani, F.; Cavalieri, R.; Chiummo, A.; Cuoco, E.; Dattilo, V.; Ferrini, F.; Fiori, I.; Genin, E.; Hemming, G.; Kasprzack, M.; Marque, J.; Mohan, M.; Nocera, F.; Paoletti, F.; Pasqualetti, A.; Ruggi, P.; Sentenac, D.; Swinkels, B.; Tacca, M.] European Gravitat Observ, I-56021 Cascina, PI, Italy.
[Ballmer, S.; Brown, D. A.; Couvares, P.; Fisher, R. P.; Harry, I. W.; Kelley, D.; Kumar, P.; Lough, J.; Mohapatra, S. R. P.; Nitz, A.; Perreca, A.; Saulson, P. R.; West, M.] Syracuse Univ, Syracuse, NY 13244 USA.
[Barsotti, L.; Bodiya, T. P.; Corbitt, T. R.; Donovan, F.; Dwyer, S.; Evans, M.; Foley, S.; Fritschel, P.; Katsavounidis, E.; Kissel, J. S.; Kwee, P.; MacInnis, M.; Mason, K.; Matichard, F.; Mavalvala, N.; Mittleman, R.; Oelker, E.; Sankar, S.; Shapiro, B.; Shoemaker, D. H.; Smith-Lefebvre, N. D.; Vaulin, R.; Waldman, S. J.; Weiss, R.; Wipf, C. C.; Zucker, M. E.] LIGO Massachusetts Inst Technol, Cambridge, MA 02139 USA.
[Barsuglia, M.; Bouhou, B.; Buy, C.; Chassande-Mottin, E.; Ward, R. L.] Univ Paris Diderot, CNRS, IN2P3, Observ Paris,Sorbonne Paris Cite,CEA Irfu,APC,Ast, F-75205 Paris 13, France.
[Bartos, I.; Belopolski, I.; Factourovich, M.; Marka, S.; Marka, Z.; Matone, L.; Murphy, D.; Raffai, P.; Tse, M.] Columbia Univ, New York, NY 10027 USA.
[Bassiri, R.; Beck, D.; Bhadbade, T.; Byer, R. L.; Clark, D. E.; DeBra, D.; Herrera, V.; Kim, N.; Kurdyumov, R.; Lantz, B.; Markosyan, A.; Roberts, M.] Stanford Univ, Stanford, CA 94305 USA.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Bulik, T.; Kowalska, I.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
[Bejger, M.; Jaranowski, P.; Rosinska, D.] CAMK PAN, PL-00716 Warsaw, Poland.
[Jaranowski, P.] Bialystok Univ, PL-15424 Bialystok, Poland.
[Krolak, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
[Benacquista, M.; Biswas, R.; Cagnoli, G.; Creighton, T. D.; Daveloza, H.; Diaz, M.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E.; Quetschke, V.; Rakhmanov, M.; Stone, R.; Stroeer, A. S.; Torres, C. V.] Univ Texas Brownsville, Brownsville, TX 78520 USA.
[Beyersdorf, P. T.; Cordier, M.] San Jose State Univ, San Jose, CA 95192 USA.
[Bilenko, I. A.; Braginsky, V. B.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L. G.; Strigin, S. E.; Vyatchanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia.
[Bizouard, M. A.; Brisson, V.; Cavalier, F.; Davier, M.; Franco, S.; Hello, P.; Kasprzack, M.; Leroy, N.; Robinet, F.; Vavoulidis, M.; Was, M.] Univ Paris 11, CNRS, IN2P3, LAL, F-91898 Orsay, France.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Blackburn, L.; Camp, J. B.; Graff, P. B.; Kanner, J. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blair, D.; Chen, X.; Chung, S.; Coward, D. M.; Danilishin, S. L.; Dumas, J. -C.; Hooper, S.; Howell, E. J.; Ju, L.; Susmithan, S.; Wen, L.; Whitcomb, S. E.; Zhao, C.] Univ Western Australia, Crawley, Washington 6009, Australia.
[Bondarescu, R.; Finn, L. S.; Menendez, D. F.; Owen, B. J.; Titsler, C.] Penn State Univ, University Pk, PA 16802 USA.
[Brillet, A.; Cleva, F.; Coulon, J. -P.; Fournier, J. -D.; Heitmann, H.; Man, N.; Pichot, M.; Regimbau, T.; Vinet, J. -Y.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice, France.
[Bondu, F.; Hayau, J. -F.] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France.
[Bonnand, R.; Cagnoli, G.; Degallaix, J.; Flaminio, R.; Franc, J.; Galimberti, M.; Granata, M.; Michel, C.; Morgado, N.; Pinard, L.; Saracco, E.; Sassolas, B.] Univ Lyon, IN2P3, CNRS, Lab Mat Avances, F-69622 Lyon, France.
[Bose, S.; Dayanga, T.; Ghosh, S.; Steplewski, S.; Talukder, D.] Washington State Univ, Pullman, WA 99164 USA.
[Bosi, L.; Gammaitoni, L.; Marchesoni, F.; Neri, I.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Gammaitoni, L.; Neri, I.; Travasso, F.] Univ Perugia, I-06123 Perugia, Italy.
[Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy.
[Branchesi, M.; Guidi, G. M.; Lorenzini, M.; Losurdo, G.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Sesto Fiorentino, Italy.
[Branchesi, M.; Cesarini, E.; Guidi, G. M.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Univ Urbino Carlo Bo, I-61029 Urbinoc, Italy.
[Brau, J. E.; Frey, R.; Harstad, E. D.; Leonor, I.; Quitzow-James, R.; Schofield, R. M. S.] Univ Oregon, Eugene, OR 97403 USA.
[Briant, T.; Cohadon, P. -F.; Heidmann, A.] Univ Paris 06, CNRS, UPMC, ENS,Lab Kastler Brossel, F-75005 Paris, France.
[Buonanno, A.; Capano, C. D.; Kanner, J. B.; Pan, Y.; Shawhan, P.; Yancey, C. C.] Univ Maryland, College Pk, MD 20742 USA.
[Burguet-Castell, J.; Gil-Casanova, S.; Husa, S.; Sintes, A. M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain.
[Cadonati, L.; Clark, J. A.; Hoak, D.; McIver, J.] Univ Massachusetts, Amherst, MA 01003 USA.
[Cannon, K.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Cao, J.; Chen, W.; Du, Z.; Li, J.; Liu, Y.; Wan, Y.; Wang, X.; Zhang, F.] Tsinghua Univ, Beijing 100084, Peoples R China.
[Caride, S.; Gustafson, R.; Meadors, G. D.; Riles, K.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Caudill, S.; Costa, C. A.; DeRosa, R.; Effler, A.; Giaime, J. A.; Gonzalez, G.; Johnson, W. W.; Kokeyama, K.; Mullavey, A.; Slutsky, J.; Sung, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Cavaglia, M.; Dietz, A.; Rankins, B.] Univ Mississippi, University, MS 38677 USA.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Chen, Y.; Hong, T.; Kaufman, K.; Miao, H.; Ott, C. D.; Somiya, K.; Thorne, K. S.; Wen, L.; Yang, H.] Caltech CaRT, Pasadena, CA 91125 USA.
[Chincarini, A.; Gemme, G.; Prato, M.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy.
[Cho, H. S.; Kim, Y. M.; Lee, C. H.] Pusan Natl Univ, Pusan 609735, South Korea.
[Chow, J.; Chua, S. S. Y.; Inta, R.; Lam, P. K.; McClelland, D. E.; Miller, J.; Mow-Lowry, C. M.; Mullavey, A.; Nguyen, T.; Scott, S. M.; Shaddock, D. A.; Slagmolen, B. J. J.; Stefszky, M.; Wade, A.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Christensen, N.; Coughlin, M.; Isogai, T.] Carleton Coll, Northfield, MN 55057 USA.
[Chung, C. T. Y.; Melatos, A.; Sammut, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
[Coccia, E.; D'Antonio, S.; Emilio, M. Di Paolo; Fafone, V.; Malvezzi, V.; Minenkov, Y.; Morgia, A.; Palladino, L.; Re, V.; Rocchi, A.; Sperandio, L.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Coccia, E.; Fafone, V.; Morgia, A.; Re, V.; Sperandio, L.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Emilio, M. Di Paolo; Palladino, L.] Univ Aquila, I-67100 Laquila, Italy.
[Addesso, P.; Conte, R.; Postiglione, F.] Univ Salerno, I-84084 Salerno, Italy.
[Costa, C. A.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Daw, E. J.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[Debreczeni, G.; Endroczi, G.; Gaspar, M. E.; Racz, I.; Vasuth, M.] RMKI, Wigner RCP, H-1121 Budapest, Hungary.
[Dhurandhar, S.; Gupta, R.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Dorsher, S.; Kandhasamy, S.; Mandic, V.; Pihlaja, M.; Prestegard, T.; Thrane, E.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Drago, M.; Prodi, G. A.] Ist Nazl Fis Nucl, Grp Collegato Trento, I-38050 Povo, Trento, Italy.
[Drago, M.; Prodi, G. A.; Yamamoto, K.] Univ Trento, I-38050 Povo, Trento, Italy.
[Taffarello, L.; Vedovato, G.; Zendri, J. -P.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Yamamoto, K.] Univ Padua, I-35131 Padua, Italy.
[Drever, R. W. P.; Harms, J.; Langley, A.] CALTECH, Pasadena, CA 91125 USA.
[Farr, B. F.; Farr, W. M.; Fazi, D.; Jang, Y. J.; Kalogera, V.; Raymond, V.; Rodriguez, C.; Yablon, J.] Northwestern Univ, Evanston, IL 60208 USA.
[Frei, M. A.; Mohapatra, S. R. P.; Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Frei, Z.; Gelencser, G.; Raffai, P.; Szeifert, G.] Eotvos Lorand Univ, H-1117 Budapest, Hungary.
[Feroz, F.; Gair, J.] Univ Cambridge, Cambridge CB2 1TN, England.
[Gergely, L. A.; Keresztes, Z.] Univ Szeged, H-6720 Szeged, Hungary.
[Greenhalgh, R. J. S.; O'Dell, J.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England.
[Gretarsson, A. M.; Jesse, E.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Hanna, C.] Perimeter Inst Theoret Phys, Toronto, ON N2L 2Y5, Canada.
[Harry, G. M.] American Univ, Washington, DC 20016 USA.
[Holtrop, M.] Univ New Hampshire, Durham, NH 03824 USA.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Kang, G.; Kim, B. K.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea.
[Kasturi, R.; Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Khazanov, E. A.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Kim, C.] Lund Observ, SE-22100 Lund, Sweden.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland.
[Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA.
[McGuire, S. C.] Southern Univ & A&M Coll, Baton Rouge, LA 70813 USA.
[Melissinos, A. C.] Univ Rochester, Rochester, NY 14627 USA.
[Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Oh, J. J.; Oh, S. H.] Natl Inst Math Sci, Taejon 305390, South Korea.
[Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
[Santostasi, G.] McNeese State Univ, Lake Charles, LA 70609 USA.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
[Pierro, V.; Pinto, I. M.; Principe, M.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
RP Aasi, J (reprint author), LIGO Calif Inst Technol, Pasadena, CA 91125 USA.
RI Puppo, Paola/J-4250-2012; CONTE, ANDREA/J-6667-2012; Parisi,
Maria/D-2817-2013; Marchesoni, Fabio/A-1920-2008; Khazanov,
Efim/B-6643-2014; Zhao, Chunnong/C-2403-2013; prodi,
giovanni/B-4398-2010; Steinlechner, Sebastian/D-5781-2013; Strigin,
Sergey/I-8337-2012; Gemme, Gianluca/C-7233-2008; Prokhorov,
Leonid/I-2953-2012; Gammaitoni, Luca/B-5375-2009; Miao,
Haixing/O-1300-2013; Salemi, Francesco/F-6988-2014; Gorodetsky,
Michael/C-5938-2008; Mitrofanov, Valery/D-8501-2012; Bell,
Angus/E-7312-2011; Bilenko, Igor/D-5172-2012; Kumar, Prem/B-6691-2009;
Losurdo, Giovanni/K-1241-2014; Lam, Ping Koy/A-5276-2008; Hild,
Stefan/A-3864-2010; Danilishin, Stefan/K-7262-2012; Canuel,
Benjamin/C-7459-2014; Lee, Chang-Hwan/B-3096-2015; Khalili,
Farit/D-8113-2012; McClelland, David/E-6765-2010; Vecchio,
Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Finn, Lee
Samuel/A-3452-2009; Sigg, Daniel/I-4308-2015; Tacca, Matteo/J-1599-2015;
Graef, Christian/J-3167-2015; Ottaway, David/J-5908-2015; Garufi,
Fabio/K-3263-2015; Neri, Igor/F-1482-2010; Chen, Yanbei/A-2604-2013;
Shaddock, Daniel/A-7534-2011; Postiglione, Fabio/O-4744-2015; Harms,
Jan/J-4359-2012; Ward, Robert/I-8032-2014; Ferrante,
Isidoro/F-1017-2012; Prato, Mirko/D-8531-2012; Travasso,
Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo,
Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Cesarini,
Elisabetta/C-4507-2017; Costa, Cesar/G-7588-2012; Chow,
Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011;
Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev,
Alexander/F-3027-2017; Vicere, Andrea/J-1742-2012; Rocchi,
Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Branchesi,
Marica/P-2296-2015; Gehring, Tobias/A-8596-2016; Strain,
Kenneth/D-5236-2011; Heidmann, Antoine/G-4295-2016; Bao,
Yiliang/G-9848-2016; Ott, Christian/G-2651-2011; mosca,
simona/I-7116-2012; Zhu, Xingjiang/E-1501-2016; Frasconi,
Franco/K-1068-2016; Pinto, Innocenzo/L-3520-2016; Howell,
Eric/H-5072-2014;
OI Puppo, Paola/0000-0003-4677-5015; Marchesoni, Fabio/0000-0001-9240-6793;
Zhao, Chunnong/0000-0001-5825-2401; prodi, giovanni/0000-0001-5256-915X;
Steinlechner, Sebastian/0000-0003-4710-8548; Gemme,
Gianluca/0000-0002-1127-7406; Gammaitoni, Luca/0000-0002-4972-7062;
Miao, Haixing/0000-0003-4101-9958; Gorodetsky,
Michael/0000-0002-5159-2742; Bell, Angus/0000-0003-1523-0821; Losurdo,
Giovanni/0000-0003-0452-746X; Lam, Ping Koy/0000-0002-4421-601X;
Danilishin, Stefan/0000-0001-7758-7493; Lee,
Chang-Hwan/0000-0003-3221-1171; McClelland, David/0000-0001-6210-5842;
Vecchio, Alberto/0000-0002-6254-1617; Finn, Lee
Samuel/0000-0002-3937-0688; Sigg, Daniel/0000-0003-4606-6526; Tacca,
Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603;
Garufi, Fabio/0000-0003-1391-6168; Neri, Igor/0000-0002-9047-9822;
Shaddock, Daniel/0000-0002-6885-3494; Postiglione,
Fabio/0000-0003-0628-3796; Kanner, Jonah/0000-0001-8115-0577;
Jaranowski, Piotr/0000-0001-8085-3414; Aulbert,
Carsten/0000-0002-1481-8319; Rover, Christian/0000-0002-6911-698X;
Milano, Leopoldo/0000-0001-9487-5876; Swinkels, Bas/0000-0002-3066-3601;
Drago, Marco/0000-0002-3738-2431; Ward, Robert/0000-0001-5503-5241;
Ricci, Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576;
Ferrante, Isidoro/0000-0002-0083-7228; Prato, Mirko/0000-0002-2188-8059;
Travasso, Flavio/0000-0002-4653-6156; Punturo,
Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338;
Cesarini, Elisabetta/0000-0001-9127-3167; 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; Vicere, Andrea/0000-0003-0624-6231;
Rocchi, Alessio/0000-0002-1382-9016; Martelli,
Filippo/0000-0003-3761-8616; Gehring, Tobias/0000-0002-4311-2593;
Strain, Kenneth/0000-0002-2066-5355; Heidmann,
Antoine/0000-0002-0784-5175; Ott, Christian/0000-0003-4993-2055; mosca,
simona/0000-0001-7869-8275; Zhu, Xingjiang/0000-0001-7049-6468;
Frasconi, Franco/0000-0003-4204-6587; Vedovato,
Gabriele/0000-0001-7226-1320; Howell, Eric/0000-0001-7891-2817; Boschi,
Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418;
Papa, M.Alessandra/0000-0002-1007-5298; Pinto, Innocenzo
M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; calloni,
enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Sorazu,
Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735; Bondu,
Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397; Del
Pozzo, Walter/0000-0003-3978-2030; O'Shaughnessy,
Richard/0000-0001-5832-8517; Vocca, Helios/0000-0002-1200-3917;
Fairhurst, Stephen/0000-0001-8480-1961; Nitz,
Alexander/0000-0002-1850-4587; 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; Addesso, Paolo/0000-0003-0895-184X; Allen,
Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Husa,
Sascha/0000-0002-0445-1971; Di Paolo Emilio,
Maurizio/0000-0002-9558-3610; Vitale, Salvatore/0000-0003-2700-0767;
PERSICHETTI, GIANLUCA/0000-0001-8424-9791; Freise,
Andreas/0000-0001-6586-9901; Guidi, Gianluca/0000-0002-3061-9870;
Pierro, Vincenzo/0000-0002-6020-5521; Coccia,
Eugenio/0000-0002-6669-5787; Hallam, Jonathan Mark/0000-0002-7087-0461;
Vetrano, Flavio/0000-0002-7523-4296; Naticchioni,
Luca/0000-0003-2918-0730; Nishizawa, Atsushi/0000-0003-3562-0990
FU United States National Science Foundation; Science and Technology
Facilities Council of the United Kingdom; Max-Planck-Society; State of
Niedersachsen/Germany [GEO600]; Italian Istituto Nazionale di Fisica
Nucleare; French Centre National de la Recherche Scientifique;
Australian Research Council; International Science Linkages program of
the Commonwealth of Australia; Council of Scientific and Industrial
Research of India; Istituto Nazionale di Fisica Nucleare of Italy;
Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia
Hisenda i Innovacio of the Govern de les Illes Balears; Foundation for
Fundamental Research on Matter; Netherlands Organisation for Scientific
Research; Polish Ministry of Science and Higher Education; FOCUS
Programme of Foundation for Polish Science; Royal Society; Scottish
Funding Council; Scottish Universities Physics Alliance; National
Aeronautics and Space Administration; National Research Foundation of
Korea; Industry Canada; Province of Ontario through the Ministry of
Economic Development and Innovation; National Science and Engineering
Research Council Canada; Carnegie Trust; Leverhulme Trust; David and
Lucile Packard Foundation; Research Corporation; Alfred P. Sloan
Foundation
FX The authors gratefully acknowledge the support of the United States
National Science Foundation for the construction and operation of the
LIGO Laboratory, the Science and Technology Facilities Council of the
United Kingdom, the Max-Planck-Society, and the State of
Niedersachsen/Germany for support of the construction and operation of
the GEO600 detector, and the Italian Istituto Nazionale di Fisica
Nucleare and the French Centre National de la Recherche Scientifique for
the construction and operation of the Virgo detector. The authors also
gratefully acknowledge the support of the research by these agencies and
by the Australian Research Council, the International Science Linkages
program of the Commonwealth of Australia, the Council of Scientific and
Industrial Research of India, the Istituto Nazionale di Fisica Nucleare
of Italy, the Spanish Ministerio de Economia y Competitividad, the
Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes
Balears, the Foundation for Fundamental Research on Matter supported by
the Netherlands Organisation for Scientific Research, the Polish
Ministry of Science and Higher Education, the FOCUS Programme of
Foundation for Polish Science, the Royal Society, the Scottish Funding
Council, the Scottish Universities Physics Alliance, the National
Aeronautics and Space Administration, the National Research Foundation
of Korea, Industry Canada and the Province of Ontario through the
Ministry of Economic Development and Innovation, the National Science
and Engineering Research Council Canada, the Carnegie Trust, the
Leverhulme Trust, the David and Lucile Packard Foundation, the Research
Corporation, and the Alfred P. Sloan Foundation.
NR 66
TC 90
Z9 90
U1 8
U2 106
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD SEP 4
PY 2013
VL 88
IS 6
AR 062001
DI 10.1103/PhysRevD.88.062001
PG 24
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 211XU
UT WOS:000323946300001
ER
PT J
AU Crawford, LS
Do, MB
Ruml, W
Hindi, H
Eldershaw, C
Zhou, R
Kuhn, L
Fromherz, MPJ
Biegelsen, D
de Kleer, J
Larner, D
AF Crawford, Lara S.
Minh Binh Do
Ruml, Wheeler
Hindi, Haitham
Eldershaw, Craig
Zhou, Rong
Kuhn, Lukas
Fromherz, Markus P. J.
Biegelsen, David
de Kleer, Johan
Larner, Daniel
TI Online Reconfigurable Machines
SO AI MAGAZINE
LA English
DT Article
ID MANUFACTURING SYSTEMS; DESIGN
AB A recent trend in intelligent machines and manufacturing has been toward reconfigurable manufacturing systems. Such systems move away from a fixed factory line executing an unchanging set of operations and toward the goal of an adaptable factory structure. The logical next challenge in this area is that of online reconfigurability. With this capability, machines can reconfigure while running, enable or disable capabilities in real time, and respond quickly to changes in the system or the environment (including faults). We propose an approach to achieving online reconfigurability based on a high level of system modularity supported by integrated, model-based planning and control software. Our software capitalizes on many advanced techniques from the artificial intelligence research community, particularly in model-based domain-independent planning and scheduling, heuristic search, and temporal resource reasoning. We describe the implementation of this design in a prototype highly modular, parallel printing system.
C1 [Crawford, Lara S.; Hindi, Haitham; Zhou, Rong; Fromherz, Markus P. J.] Palo Alto Res Ctr, ISL, Palo Alto, CA 94304 USA.
[Minh Binh Do] SGT Inc, Greenbelt, MD USA.
[Minh Binh Do] NASA, Ames Res Ctr, Planning & Scheduling Grp, Washington, DC USA.
[Ruml, Wheeler] Univ New Hampshire, Durham, NH 03824 USA.
[Ruml, Wheeler] Palo Alto Res Ctr, Palo Alto, CA USA.
[Hindi, Haitham] Walmart Labs, San Francisco, CA 94118 USA.
[Eldershaw, Craig] Palo Alto Res Ctr, Hardware Syst Lab, Palo Alto, CA USA.
[Kuhn, Lukas] Palo Alto Res Ctr, Embedded Reasoning Area, Palo Alto, CA USA.
RP Crawford, LS (reprint author), Palo Alto Res Ctr, ISL, Palo Alto, CA 94304 USA.
FU Xerox
FX The authors would like to thank all of our many current and former
colleagues at PARC and Xerox who have contributed to this project.
Special thanks to Bob Lofthus and Martin Krucinski. This work was funded
by Xerox.
NR 38
TC 0
Z9 0
U1 3
U2 5
PU AMER ASSOC ARTIFICIAL INTELL
PI MENLO PK
PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA
SN 0738-4602
J9 AI MAG
JI AI Mag.
PD FAL
PY 2013
VL 34
IS 3
BP 73
EP 88
PG 16
WC Computer Science, Artificial Intelligence
SC Computer Science
GA AI5FX
UT WOS:000336891900006
ER
PT J
AU Sutliff, DL
Jones, MG
Hartley, TC
AF Sutliff, Daniel L.
Jones, Michael G.
Hartley, Thomas C.
TI High-Speed Turbofan Noise Reduction Using Foam-Metal Liner
Over-the-Rotor
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 47th AIAA Aerospace Sciences Meeting and Exhibit Including the New
Horizons Forum and Aerospace Exposition
CY JAN 05-08, 2009
CL Orlando, FL
SP AIAA
ID ACOUSTIC PROPERTIES
AB A Williams International FJ44-3A turbofan engine was used to demonstrate the high-speed fan noise reduction potential of a foam-metal liner installed in close proximity to the fan rotor. The engine was tested in the NASA Glenn Research Center's Aeroacoustic Propulsion Laboratory. Two foam-metal liner designs were tested and compared to the hardwall baseline. Traditional single degree-of-freedom liner designs were also evaluated to provide a comparison to the state-of-the art design. This report presents the test setup and documents the test conditions. Far-field acoustic levels and limited engine performance results are also presented. The results show that the foam-metal liner achieved up to 5 dB of attenuation in the forward-quadrant radiated-acoustic power levels, which is equivalent to the traditional single degree-of-freedom liner design. Modest changes in engine performance were noted.
C1 [Sutliff, Daniel L.] NASA, John H Glenn Res Ctr Lewis Field, Acoust Branch, Cleveland, OH 44135 USA.
[Jones, Michael G.] NASA, Langley Res Ctr, Res & Technol Directorate, Struct Acoust Branch, Hampton, VA USA.
[Hartley, Thomas C.] Williams Int, Compress Team, Walled Lake, MI 48390 USA.
RP Sutliff, DL (reprint author), NASA, John H Glenn Res Ctr Lewis Field, Acoust Branch, Cleveland, OH 44135 USA.
NR 16
TC 3
Z9 3
U1 3
U2 5
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 SEP-OCT
PY 2013
VL 50
IS 5
BP 1491
EP 1503
DI 10.2514/1.C032021
PG 13
WC Engineering, Aerospace
SC Engineering
GA AA8VK
UT WOS:000331372900014
ER
PT J
AU Chen, YK
Gokcen, T
AF Chen, Yih-Kanq
Goekcen, Tahir
TI Effect of Nonequilibrium Surface Thermochemistry in Simulation of
Carbon-Based Ablators
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 43rd AIAA Thermophysics Conference
CY JUN 25-28, 2012
CL New Orleans, LA
SP AIAA
ID THERMAL RESPONSE; SHAPE CHANGE; ABLATION; MODEL
AB This study demonstrates that coupling of a material thermal-response code and a flow solver using a nonequilibrium gas/surface-interaction model provides time-accurate solutions for the multidimensional ablation of carbon-based charring ablators. The material thermal-response code used in this study is the two-dimensional implicit thermal response and ablation program, which predicts the charring-material thermal response and shape change on hypersonic space vehicles. Its governing equations include total energy balance, pyrolysis-gas mass conservation, and a three-component decomposition model. The flow code solves the reacting Navier-Stokes equations using the data-parallel-line-relaxation method. Loose coupling between the material-response and flow codes is performed by solving the surface mass balance in the flow code and the surface energy balance in the material-response code. Thus, the material surface recession is predicted by finite rate gas/surface-interaction boundary conditions implemented in the flow code, and the surface temperature and the pyrolysis-gas injection rate are computed in the material-response code. Two sets of nonequilibrium gas/surface-interaction chemistry between air and the carbon surface are studied. Coupled fluid-material-response analyses of stagnation tests conducted at the NASA Ames Research Center arcjet facilities are considered. The ablating material used in these arcjet tests was phenolic impregnated carbon ablator. Computational predictions of in-depth material thermal response and surface recession are in excellent agreement with the data for conditions in which carbon recession rate is limited by species diffusion.
C1 [Chen, Yih-Kanq] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
[Goekcen, Tahir] NASA, Ames Res Ctr, ERC Inc, Moffett Field, CA 94035 USA.
RP Chen, YK (reprint author), NASA, Ames Res Ctr, Thermal Protect Mat Branch, MS 234-1, Moffett Field, CA 94035 USA.
NR 18
TC 2
Z9 4
U1 2
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 SEP-OCT
PY 2013
VL 50
IS 5
BP 917
EP 926
DI 10.2514/1.A32451
PG 10
WC Engineering, Aerospace
SC Engineering
GA AA8VP
UT WOS:000331373400001
ER
PT J
AU Hollis, BR
Hollingsworth, KE
AF Hollis, Brian R.
Hollingsworth, Kevin E.
TI Laminar, Transitional, and Turbulent Heating on Mid Lift-to-Drag Ratio
Entry Vehicles
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 42nd AIAA Fluid Dynamics Conference and Exhibit
CY JUN 25-28, 2012
CL New Orleans, LA
SP AIAA
AB The boundary-layer transition characteristics and convective aeroheating levels on mid lift-to-drag ratio entry vehicle configurations have been studied through wind-tunnel testing. Several configurations were investigated, including elliptically blunted cylinders with both circular and elliptically flattened cross sections, biconic geometries based on launch vehicle dual-use shrouds, and parametrically optimized analytic geometries. Vehicles of this class have been proposed for high-mass Mars missions, such as sample return and crewed exploration, for which the conventional sphere-cone entry-vehicle geometries of previous Mars missions are insufficient. Testing was conducted at Mach 6 over a range of Reynolds numbers sufficient to generate laminar, transitional, and turbulent flow. Transition onset locations, both straight-line and cross-flow, and heating rates were obtained through global phosphor thermography. Supporting computations were performed to obtain heating rates for comparison with the data. Laminar data and predictions agreed to well within the experimental uncertainty. Fully turbulent data and predictions also agreed well. However, in transitional flow regions, greater differences were observed.
C1 [Hollis, Brian R.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
[Hollingsworth, Kevin E.] Aerosp Comp Inc, Superson Hyperson Test Branch, Hampton, VA 23681 USA.
RP Hollis, BR (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
NR 19
TC 1
Z9 1
U1 0
U2 3
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 SEP-OCT
PY 2013
VL 50
IS 5
BP 937
EP 949
DI 10.2514/1.A32458
PG 13
WC Engineering, Aerospace
SC Engineering
GA AA8VP
UT WOS:000331373400003
ER
PT J
AU Panda, J
Mosher, R
AF Panda, J.
Mosher, R.
TI Microphone Phased Array to Identify Liftoff Noise Sources in Model-Scale
Tests
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 50th AIAA Aerospace Sciences Meeting and Exhibit including the New
Horizons Forum and Aerospace Exposition
CY JAN 06-13, 2012
CL Nashville, TN
SP AIAA, US AF Off Sci Res
AB A 70-microphone phased array, protected to withstand the harsh environment of a rocket test facility, was used to identify noise sources in the Ares I Scale Model Acoustics Test. In the unobstructed burn of a single solid rocket motor, the free-flowing plume itself was found to make a long noise source. The scenario changed completely in launch configurations where a 5%-scale model of the Ares I vehicle was tested in static firings. It was found that the impingement by the plume on various regions of the launch pad constituted the primary noise sources. The scenario is very different from current models, which assume that the plume itself is the noise source and do not account for impingement sources. As expected, the addition of water in the trench and the hole for the plume passage attenuated the associated noise sources. Water injection on the top of the pad ("rainbird") was found to attenuate only the peripheral sources around the primary plume impingement zone. The noise maps suggest that the minimization of impingement by reducing vehicle drift, reducing plume spillage via increasing the size of the hole, and covering-up leakage paths for the sound waves from the trench will attenuate the liftoff acoustics level.
C1 [Panda, J.] NASA, Ames Res Ctr, Expt Aerophys Branch, Moffett Field, CA 94035 USA.
[Mosher, R.] Aerosp Comp Inc, Expt Aerophys Branch, Mountain View, CA 94043 USA.
RP Panda, J (reprint author), NASA, Ames Res Ctr, Expt Aerophys Branch, Moffett Field, CA 94035 USA.
NR 16
TC 3
Z9 3
U1 1
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 SEP-OCT
PY 2013
VL 50
IS 5
BP 1002
EP 1012
DI 10.2514/1.A32433
PG 11
WC Engineering, Aerospace
SC Engineering
GA AA8VP
UT WOS:000331373400008
ER
PT J
AU Smith, TB
Harrigan, RJ
Kirschel, ANG
Buermann, W
Saatchi, S
Blumstein, DT
de Kort, SR
Slabbekoorn, H
AF Smith, Thomas B.
Harrigan, Ryan J.
Kirschel, Alexander N. G.
Buermann, Wolfgang
Saatchi, Sassan
Blumstein, Daniel T.
de Kort, Selvino R.
Slabbekoorn, Hans
TI Predicting bird song from space
SO EVOLUTIONARY APPLICATIONS
LA English
DT Article
DE anthropogenic effects; avian song; behavioral ecology; random forests;
remote sensing; reproductive isolation; spatial heterogeneity
ID URBAN NOISE; BEHAVIORAL MECHANISM; ACOUSTIC-SIGNALS; GREAT TITS; FOREST;
DIVERGENCE; BIODIVERSITY; CONSEQUENCES; SPECIATION; SELECTION
AB Environmentally imposed selection pressures are well known to shape animal signals. Changes in these signals can result in recognition mismatches between individuals living in different habitats, leading to reproductive divergence and speciation. For example, numerous studies have shown that differences in avian song may be a potent prezygotic isolating mechanism. Typically, however, detailed studies of environmental pressures on variation in animal behavior have been conducted only at small spatial scales. Here, we use remote-sensing data to predict animal behavior, in this case, bird song, across vast spatial scales. We use remotely sensed data to predict the song characteristics of the little greenbul (Andropadus virens), a widely distributed African passerine, found across secondary and mature rainforest habitats and the rainforest-savanna ecotone. Satellite data that captured ecosystem structure and function explained up to 66% of the variation in song characteristics. Song differences observed across habitats, including those between human-altered and mature rainforest, have the potential to lead to reproductive divergence, and highlight the impacts that both natural and anthropogenic change may have on natural populations. Our approach offers a novel means to examine the ecological correlates of animal behavior across large geographic areas with potential applications to both evolutionary and conservation biology.
C1 [Smith, Thomas B.; Kirschel, Alexander N. G.; Blumstein, Daniel T.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Smith, Thomas B.; Harrigan, Ryan J.; Kirschel, Alexander N. G.; Buermann, Wolfgang; Saatchi, Sassan; Blumstein, Daniel T.; Slabbekoorn, Hans] Univ Calif Los Angeles, Inst,Environm & Sustainabil, Ctr Trop Res, Los Angeles, CA 90095 USA.
[Kirschel, Alexander N. G.] Univ Cyprus Nicosia, Dept Biol Sci, Nicosia, Cyprus.
[Kirschel, Alexander N. G.] Univ Oxford, Dept Zool, Edward Grey Inst, Oxford OX1 3PS, England.
[Saatchi, Sassan] Calif Inst Technol Pasadena, Jet Prop Lab, Pasadena, CA USA.
[de Kort, Selvino R.] Manchester Metropolitan Univ Manchester, Sch Sci & Environm, Div Biol & Conservat Ecol, Manchester, Lancs, England.
[Slabbekoorn, Hans] Leiden Univ, Inst Biol, Leiden, Netherlands.
RP Smith, TB (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, 621 Charles E Young Dr South, Los Angeles, CA 90095 USA.
EM tbsmith@ucla.edu
OI Kirschel, Alexander/0000-0003-4379-7956; Blumstein,
Daniel/0000-0001-5793-9244
FU National Geographic Society; NERC [GR3/85519A9]; Veneklasen Research
Foundation; Royal Society [571310.V703]; NSF [BSR 88-17336,
IRCEB9977072]; NASA [IDS/03-0169-0347]
FX We thank the government of the Republic of Cameroon for permission to
conduct the field research and our many field assistants over the years.
We thank J. A. Endler, P. M. Narins, W. F. Laurance, and B. Larison for
comments on the manuscript. The research was supported by grants from
the National Geographic Society, NERC (GR3/85519A9), Veneklasen Research
Foundation, Royal Society (571310.V703), NSF (BSR 88-17336 and
IRCEB9977072), and NASA (IDS/03-0169-0347).
NR 35
TC 6
Z9 6
U1 1
U2 47
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1752-4571
J9 EVOL APPL
JI Evol. Appl.
PD SEP
PY 2013
VL 6
IS 6
BP 865
EP 874
DI 10.1111/eva.12072
PG 10
WC Evolutionary Biology
SC Evolutionary Biology
GA 296IH
UT WOS:000330178000001
PM 24062797
ER
PT J
AU Brown, GV
Beilmann, C
Bernitt, S
Clementson, J
Eberle, S
Epp, SW
Graf, A
Hell, N
Kelley, RL
Kilbourne, CA
Kubicek, K
Leutenegger, MA
Mackel, V
Porter, FS
Rudolph, JK
Simon, MC
Steinbrugge, R
Trabert, E
Ullrich, J
Lopez-Urrutia, JRC
Beiersdorfer, P
AF Brown, G. V.
Beilmann, C.
Bernitt, S.
Clementson, J.
Eberle, S.
Epp, S. W.
Graf, A.
Hell, N.
Kelley, R. L.
Kilbourne, C. A.
Kubicek, K.
Leutenegger, M. A.
Maeckel, V.
Porter, F. S.
Rudolph, J. K.
Simon, M. C.
Steinbruegge, R.
Traebert, E.
Ullrich, J.
Lopez-Urrutia, J. R. Crespo
Beiersdorfer, P.
TI Studies of highly charged iron ions using electron beam ion traps for
interpreting astrophysical spectra
SO PHYSICA SCRIPTA
LA English
DT Article; Proceedings Paper
CT 16th International Conference on the Physics of Highly Charged Ions
(HCI)
CY SEP 02-07, 2012
CL Ruprecht Karls Univ, Heidelberg, GERMANY
SP CAEN, Oerlikon Leybold Vacuum, RoentDek Handels, Struck Innovat Syst
HO Ruprecht Karls Univ
ID FE XVI; SPECTROMETER; EMISSION; SPECTROSCOPY; EXCHANGE; EBIT
AB For over a decade, the x-ray astrophysics community has enjoyed a fruitful epoch of discovery largely as a result of the successful launch and operation of the high resolution, high sensitivity spectrometers on board the Chandra, XMM-Newton and Suzaku x-ray observatories. With the launch of the x-ray calorimeter spectrometer on the Astro-H x-ray observatory in 2014, the diagnostic power of high resolution spectroscopy will be extended to some of the hottest, largest and most exotic objects in our Universe. The diagnostic utility of these spectrometers is directly coupled to, and often limited by, our understanding of the x-ray production mechanisms associated with the highly charged ions present in the astrophysical source. To provide reliable benchmarks of theoretical calculations and to address specific problems facing the x-ray astrophysics community, electron beam ion traps have been used in laboratory astrophysics experiments to study the x-ray signatures of highly charged ions. A brief overview of the EBIT-I electron beam ion trap operated at Lawrence Livermore National Laboratory and the Max-Planck-Institut fur Kernphysik's FLASH-EBIT operated at third and fourth generation advanced light sources, including a discussion of some of the results are presented.
C1 [Brown, G. V.; Clementson, J.; Graf, A.; Traebert, E.; Beiersdorfer, P.] Lawrence Livermore Natl Lab, Div Phys, Livermore, CA 94550 USA.
[Beilmann, C.; Bernitt, S.; Eberle, S.; Kubicek, K.; Maeckel, V.; Rudolph, J. K.; Steinbruegge, R.; Ullrich, J.; Lopez-Urrutia, J. R. Crespo] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Epp, S. W.] Ctr Free Electron Laser Sci, Max Planck Adv Study Grp, D-22607 Hamburg, Germany.
[Hell, N.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte Bamberg & Erlangen Ctr, D-96049 Bamberg, Germany.
[Kelley, R. L.; Kilbourne, C. A.; Leutenegger, M. A.; Porter, F. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Leutenegger, M. A.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
[Rudolph, J. K.] Univ Giessen, Inst Atom & Mol Phys, D-35392 Giessen, Germany.
[Simon, M. C.] TRIUMF, Vancouver, BC V6T 2A3, Canada.
RP Brown, GV (reprint author), Lawrence Livermore Natl Lab, Div Phys, Livermore, CA 94550 USA.
EM brown86@llnl.gov
RI Porter, Frederick/D-3501-2012; Crespo Lopez-Urrutia, Jose
R./F-7069-2011; Simon, Martin/I-5384-2012;
OI Porter, Frederick/0000-0002-6374-1119; Crespo Lopez-Urrutia, Jose
R./0000-0002-2937-8037; Hell, Natalie/0000-0003-3057-1536; Epp,
Sascha/0000-0001-6366-9113
NR 27
TC 1
Z9 1
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0031-8949
EI 1402-4896
J9 PHYS SCRIPTA
JI Phys. Scr.
PD SEP
PY 2013
VL T156
AR 014001
DI 10.1088/0031-8949/2013/T156/014001
PG 3
WC Physics, Multidisciplinary
SC Physics
GA 280IP
UT WOS:000329022300002
ER
PT J
AU Hell, N
Miskovicova, I
Brown, GV
Wilms, J
Clementson, J
Hanke, M
Beiersdorfer, P
Liedahl, D
Pottschmidt, K
Porter, FS
Kilbourne, CA
Kelley, RL
Nowak, MA
Schulz, NS
AF Hell, Natalie
Miskovicova, I.
Brown, G. V.
Wilms, J.
Clementson, J.
Hanke, M.
Beiersdorfer, P.
Liedahl, D.
Pottschmidt, K.
Porter, F. S.
Kilbourne, C. A.
Kelley, R. L.
Nowak, M. A.
Schulz, N. S.
TI Low charge states of Si and S in Cygnus X-1
SO PHYSICA SCRIPTA
LA English
DT Article; Proceedings Paper
CT 16th International Conference on the Physics of Highly Charged Ions
(HCI)
CY SEP 02-07, 2012
CL Ruprecht Karls Univ, Heidelberg, GERMANY
SP CAEN, Oerlikon Leybold Vacuum, RoentDek Handels, Struck Innovat Syst
HO Ruprecht Karls Univ
ID RAY; CHANDRA; WIND
AB Strong, relatively short, absorption dips have been observed in the x-ray light curves measured from the high mass x-ray binary system Cygnus X-1. With increasing strength of the dips, which are believed to be caused by 'clumps' of cold material present in the stellar wind of Cyg X-1's companion star, K-shell absorption lines in L-shell ions of Si and S develop. To determine the bulk motion of the clumps via the Doppler shifts of these lines with high accuracy, we measured their reference energies using the Lawrence Livermore National Laboratory electron beam ion trap EBIT-I and EBIT Calorimeter Spectrometer. Our findings-shifts consistent with zero velocity of the absorber throughout all ionization states at orbital phase zero-provide evidence for an onion-like ion structure of the clumps.
C1 [Hell, Natalie; Miskovicova, I.; Wilms, J.; Hanke, M.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany.
[Hell, Natalie; Brown, G. V.; Clementson, J.; Beiersdorfer, P.; Liedahl, D.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Pottschmidt, K.; Porter, F. S.; Kilbourne, C. A.; Kelley, R. L.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
[Nowak, M. A.; Schulz, N. S.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
RP Hell, N (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, Sternwartstr 7, D-96049 Bamberg, Germany.
EM natalie.hell@sternwarte.uni-erlangen.de
RI Wilms, Joern/C-8116-2013; Porter, Frederick/D-3501-2012;
OI Wilms, Joern/0000-0003-2065-5410; Porter, Frederick/0000-0002-6374-1119;
Hell, Natalie/0000-0003-3057-1536
NR 12
TC 6
Z9 6
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0031-8949
EI 1402-4896
J9 PHYS SCRIPTA
JI Phys. Scr.
PD SEP
PY 2013
VL T156
AR 014008
DI 10.1088/0031-8949/2013/T156/014008
PG 3
WC Physics, Multidisciplinary
SC Physics
GA 280IP
UT WOS:000329022300009
ER
PT J
AU Kraft-Bermuth, S
Andrianov, V
Bleile, A
Echler, A
Egelhof, P
Grabitz, P
Ilieva, S
Kilbourne, C
Kiselev, O
McCammon, D
Meier, J
AF Kraft-Bermuth, S.
Andrianov, V.
Bleile, A.
Echler, A.
Egelhof, P.
Grabitz, P.
Ilieva, S.
Kilbourne, C.
Kiselev, O.
McCammon, D.
Meier, J.
TI High-precision x-ray spectroscopy of highly charged ions with
microcalorimeters
SO PHYSICA SCRIPTA
LA English
DT Article; Proceedings Paper
CT 16th International Conference on the Physics of Highly Charged Ions
(HCI)
CY SEP 02-07, 2012
CL Ruprecht Karls Univ, Heidelberg, GERMANY
SP CAEN, Oerlikon Leybold Vacuum, RoentDek Handels, Struck Innovat Syst
HO Ruprecht Karls Univ
ID LAMB SHIFT MEASUREMENTS; HYDROGEN-LIKE; HEAVY-IONS
AB The precise determination of the energy of the Lyman alpha 1 and alpha 2 lines in hydrogen-like heavy ions provides a sensitive test of quantum electrodynamics in very strong Coulomb fields. To improve the experimental precision, the new detector concept of microcalorimeters is now exploited for such measurements. Such detectors consist of compensated-doped silicon thermistors and Pb or Sn absorbers to obtain high quantum efficiency in the energy range of 40-70 keV, where the Doppler-shifted Lyman lines are located. For the first time, a microcalorimeter was applied in an experiment to precisely determine the transition energy of the Lyman lines of lead ions at the experimental storage ring at GSI. The energy of the Ly alpha 1 line E(Ly-alpha 1,Pb-207(81+)) = (77937+/-12(stat)+/-25(syst)) eV agrees within error bars with theoretical predictions. To improve the experimental precision, a new detector array with more pixels and better energy resolution was equipped and successfully applied in an experiment to determine the Lyman-alpha lines of gold ions Au-197(78+).
C1 [Kraft-Bermuth, S.] Univ Giessen, Inst Atom Phys, D-35390 Giessen, Germany.
[Andrianov, V.; Bleile, A.; Echler, A.; Egelhof, P.; Grabitz, P.; Ilieva, S.; Kiselev, O.; Meier, J.] GSI Helmholtz Ctr Heavy Ion Res, Darmstadt, Germany.
[Andrianov, V.] Moscow MV Lomonosov State Univ, Inst Nucl Phys, Moscow, Russia.
[Bleile, A.; Echler, A.; Egelhof, P.; Grabitz, P.] Johannes Gutenberg Univ Mainz, Inst Phys, Mainz, Germany.
[Kilbourne, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McCammon, D.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
RP Kraft-Bermuth, S (reprint author), Univ Giessen, Inst Atom Phys, D-35390 Giessen, Germany.
EM saskia.kraft-bermuth@iamp.physik.uni-giessen.de
RI Kraft-Bermuth, Saskia/G-4007-2012
OI Kraft-Bermuth, Saskia/0000-0002-0864-7912
NR 8
TC 3
Z9 3
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0031-8949
EI 1402-4896
J9 PHYS SCRIPTA
JI Phys. Scr.
PD SEP
PY 2013
VL T156
AR 014022
DI 10.1088/0031-8949/2013/T156/014022
PG 3
WC Physics, Multidisciplinary
SC Physics
GA 280IP
UT WOS:000329022300023
ER
PT J
AU Leutenegger, MA
Betancourt-Martinez, GL
Beiersdorfer, P
Brown, GV
Kelley, RL
Kilbourne, CA
Porter, FS
AF Leutenegger, Maurice A.
Betancourt-Martinez, Gabriele L.
Beiersdorfer, Peter
Brown, Gregory V.
Kelley, Richard L.
Kilbourne, Caroline A.
Porter, F. Scott
TI Charge exchange measurements with an x-ray calorimeter at an electron
beam ion trap
SO PHYSICA SCRIPTA
LA English
DT Article; Proceedings Paper
CT 16th International Conference on the Physics of Highly Charged Ions
(HCI)
CY SEP 02-07, 2012
CL Ruprecht Karls Univ, Heidelberg, GERMANY
SP CAEN, Oerlikon Leybold Vacuum, RoentDek Handels, Struck Innovat Syst
HO Ruprecht Karls Univ
ID EXCITED-STATES; TOKAMAK; POPULATION; PLASMAS
AB We present K-shell x-ray spectra of highly ionized Mg acquired with the EBIT calorimeter spectrometer at a resolution of 4.5 eV in charge exchange recombination experiments using the LLNL EBIT-I electron beam ion trap. We measured the Doppler width of Mg11+ Ly alpha in the same experiments using a high resolution crystal spectrometer, giving an estimate of the ion temperature. We find hardness ratios for Mg11+ ranging from 0.6 to 1.6, depending on the neutral gas target. In most of the experiments, the ion temperature was similar to 10-15 eV amu(-1), indicating that the variations in hardness ratio are intrinsic to the choice of neutral target gas, and are not simply a consequence of variations in the collision velocity resulting from evaporative cooling of the trapped ions. The spectral variations show that high resolution x-ray spectroscopy is highly diagnostic of charge exchange reactions, but requires well-developed theory to interpret.
C1 [Leutenegger, Maurice A.; Betancourt-Martinez, Gabriele L.; Kelley, Richard L.; Kilbourne, Caroline A.; Porter, F. Scott] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Leutenegger, Maurice A.] CRESST, Baltimore, MD 21250 USA.
[Leutenegger, Maurice A.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Betancourt-Martinez, Gabriele L.] CRESST, College Pk, MD 20742 USA.
[Betancourt-Martinez, Gabriele L.] Univ Maryland, College Pk, MD 20742 USA.
[Beiersdorfer, Peter; Brown, Gregory V.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
RP Leutenegger, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM maurice.a.leutenegger@nasa.gov
RI Porter, Frederick/D-3501-2012
OI Porter, Frederick/0000-0002-6374-1119
NR 19
TC 2
Z9 2
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0031-8949
EI 1402-4896
J9 PHYS SCRIPTA
JI Phys. Scr.
PD SEP
PY 2013
VL T156
AR 014006
DI 10.1088/0031-8949/2013/T156/014006
PG 4
WC Physics, Multidisciplinary
SC Physics
GA 280IP
UT WOS:000329022300007
ER
PT J
AU Bhatt, US
Walker, DA
Raynolds, MK
Bieniek, PA
Epstein, HE
Comiso, JC
Pinzon, JE
Tucker, CJ
Polyakov, IV
AF Bhatt, Uma S.
Walker, Donald A.
Raynolds, Martha K.
Bieniek, Peter A.
Epstein, Howard E.
Comiso, Josefino C.
Pinzon, Jorge E.
Tucker, Compton J.
Polyakov, Igor V.
TI Recent Declines in Warming and Vegetation Greening Trends over
Pan-Arctic Tundra
SO REMOTE SENSING
LA English
DT Article
DE AVHRR NDVI3g; tundra vegetation; climate variability; sea ice; Arctic
ID NORTHERN HIGH-LATITUDES; NDVI TIME-SERIES; SEA-ICE EXTENT;
SURFACE-TEMPERATURE; POLAR AMPLIFICATION; SHRUB EXPANSION;
AIR-TEMPERATURE; ALASKA; HETEROGENEITY; ECOSYSTEMS
AB Vegetation productivity trends for the Arctic tundra are updated for the 1982-2011 period and examined in the context of land surface temperatures and coastal sea ice. Understanding mechanistic links between vegetation and climate parameters contributes to model advancements that are necessary for improving climate projections. This study employs remote sensing data: Global Inventory Modeling and Mapping Studies (GIMMS) Maximum Normalized Difference Vegetation Index (MaxNDVI), Special Sensor Microwave Imager (SSM/I) sea-ice concentrations, and Advanced Very High Resolution Radiometer (AVHRR) radiometric surface temperatures. Spring sea ice is declining everywhere except in the Bering Sea, while summer open water area is increasing throughout the Arctic. Summer Warmth Index (SWIsum of degree months above freezing) trends from 1982 to 2011 are positive around Beringia but are negative over Eurasia from the Barents to the Laptev Seas and in parts of northern Canada. Eastern North America continues to show increased summer warmth and a corresponding steady increase in MaxNDVI. Positive MaxNDVI trends from 1982 to 2011 are generally weaker compared to trends from 1982-2008. So to better understand the changing trends, break points in the time series were quantified using the Breakfit algorithm. The most notable break points identify declines in SWI since 2003 in Eurasia and 1998 in Western North America. The Time Integrated NDVI (TI-NDVI, sum of the biweekly growing season values of MaxNDVI) has declined since 2005 in Eurasia, consistent with SWI declines. Summer (June-August) sea level pressure (slp) averages from 1999-2011 were compared to those from 1982-1998 to reveal higher slp over Greenland and the western Arctic and generally lower pressure over the continental Arctic in the recent period. This suggests that the large-scale circulation is likely a key contributor to the cooler temperatures over Eurasia through increased summer cloud cover and warming in Eastern North America from more cloud-free skies.
C1 [Bhatt, Uma S.; Bieniek, Peter A.] Univ Alaska Fairbanks, Inst Geophys, Dept Atmospher Sci, Coll Nat Sci & Math, Fairbanks, AK 99775 USA.
[Walker, Donald A.; Raynolds, Martha K.] Univ Alaska Fairbanks, Inst Arctic Biol, Dept Biol & Wildlife, Coll Nat Sci & Math, Fairbanks, AK 99775 USA.
[Bieniek, Peter A.; Polyakov, Igor V.] Coll Nat Sci & Math, Dept Atmospher Sci, Int Arctic Res Ctr, Fairbanks, AK 99775 USA.
[Epstein, Howard E.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA.
[Comiso, Josefino C.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA.
[Pinzon, Jorge E.; Tucker, Compton J.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
RP Bhatt, US (reprint author), Univ Alaska Fairbanks, Inst Geophys, Dept Atmospher Sci, Coll Nat Sci & Math, 903 Koyukuk Dr, Fairbanks, AK 99775 USA.
EM usbhatt@alaska.edu; dawalker@alaska.edu; mkraynolds@alaska.edu;
pbieniek@alaska.edu; hee2b@virginia.edu; josefino.c.comiso@nasa.gov;
jorge.e.pinzon@nasa.gov; compton.j.tucker@nasa.gov; igor@iarc.uaf.edu
FU [NSF ANS-0732885]; [NSF ARC-0902175]
FX This study was supported by grants NSF ANS-0732885, NSF ARC-0902175,
NASA Land Cover Land Use Change on the Yamal Peninsula. This work
benefitted from conversations with Ross Brown, Chris Derksen, David
Robinson and Walt Meier. Manfred Mudelsee is thanked for sharing his
FORTRAN code for the BREAKFIT programs and providing assistance with
interpreting results. We thank four anonymous reviewers for their
contributions in greatly improving this paper.
NR 76
TC 41
Z9 41
U1 14
U2 109
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD SEP
PY 2013
VL 5
IS 9
BP 4229
EP 4254
DI 10.3390/rs5094229
PG 26
WC Remote Sensing
SC Remote Sensing
GA 274NN
UT WOS:000328613300005
ER
PT J
AU Nelson, DL
Garay, MJ
Kahn, RA
Dunst, BA
AF Nelson, David L.
Garay, Michael J.
Kahn, Ralph A.
Dunst, Ben A.
TI Stereoscopic Height and Wind Retrievals for Aerosol Plumes with the MISR
INteractive eXplorer (MINX)
SO REMOTE SENSING
LA English
DT Article
DE aerosol sensing; MINX; MISR; plume height; stereoscopic retrieval
ID IMAGING SPECTRORADIOMETER MISR; CLOUD-TOP HEIGHTS; MODIS; PERFORMANCE;
SENSITIVITY; INSTRUMENT; SATELLITES; TRANSPORT; PRODUCTS; ERUPTION
AB The Multi-angle Imaging SpectroRadiometer (MISR) instrument aboard the Terra satellite acquires imagery at 275-m resolution at nine angles ranging from 0 degrees (nadir) to 70 degrees off-nadir. This multi-angle capability facilitates the stereoscopic retrieval of heights and motion vectors for clouds and aerosol plumes. MISR's operational stereo product uses this capability to retrieve cloud heights and winds for every satellite orbit, yielding global coverage every nine days. The MISR INteractive eXplorer (MINX) visualization and analysis tool complements the operational stereo product by providing users the ability to retrieve heights and winds locally for detailed studies of smoke, dust and volcanic ash plumes, as well as clouds, at higher spatial resolution and with greater precision than is possible with the operational product or with other space-based, passive, remote sensing instruments. This ability to investigate plume geometry and dynamics is becoming increasingly important as climate and air quality studies require greater knowledge about the injection of aerosols and the location of clouds within the atmosphere. MINX incorporates features that allow users to customize their stereo retrievals for optimum results under varying aerosol and underlying surface conditions. This paper discusses the stereo retrieval algorithms and retrieval options in MINX, and provides appropriate examples to explain how the program can be used to achieve the best results.
C1 [Nelson, David L.] Raytheon Co, Pasadena, CA 91101 USA.
[Garay, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kahn, Ralph A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dunst, Ben A.] Univ Calif Los Angeles, Mech & Aerosp Engn Dept, Los Angeles, CA 90095 USA.
RP Nelson, DL (reprint author), Raytheon Co, Pasadena, CA 91101 USA.
EM David.L.Nelson@jpl.nasa.gov; Michael.J.Garay@jpl.nasa.gov;
Ralph.Kahn@nasa.gov; bendunst@ucla.edu
RI Kahn, Ralph/D-5371-2012
OI Kahn, Ralph/0000-0002-5234-6359
FU NASA; NASA Goddard Space Flight Center; NASA Earth Sciences Atmospheric
Composition Modeling and Analysis Program
FX The authors thank D. J. Diner, principal investigator for the MISR
investigation, for his support of the Plume Height Project. We also
thank V. Jovanovic for leading the development of the georectified MISR
image products that make this project possible. Finally, we thank E. G.
Hansen, MISR project manager, for his support of MINX development. This
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA and at the NASA
Goddard Space Flight Center. The work of R. Kahn is also supported by
the NASA Earth Sciences Atmospheric Composition Modeling and Analysis
Program under R. Eckman.
NR 50
TC 19
Z9 19
U1 2
U2 11
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD SEP
PY 2013
VL 5
IS 9
BP 4593
EP 4628
DI 10.3390/rs5094593
PG 36
WC Remote Sensing
SC Remote Sensing
GA 274NN
UT WOS:000328613300021
ER
PT J
AU Sears, DWG
AF Sears, Derek W. G.
TI Oral Histories in Meteoritics and Planetary Science-XXI: Donald Burnett
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID SOLAR-WIND; ISOTOPIC COMPOSITION; ORDINARY CHONDRITES; ABUNDANCES;
SAMPLES; SYSTEM
AB In this interview, Donald Burnett (Fig.1) describes how he applied to the University of Chicago, with considerable support from his father, where he took classes from Harold Urey and was inspired by Ed Anders to pursue a career in nuclear chemistry and, later, cosmochemistry. As a graduate student at the University of California at Berkeley, Don learned to use charged-particle tracks as a detector for radioactive nuclei, a technique that he applied to a wide variety of problems over the next 20 years, including the neutron profile probe that was deployed on the Moon. After a one-year postdoc with William Fowler at the California Institute of Technology, he became involved with Jerry Wasserburg, who ultimately obtained a faculty position for him in the Geology Division. Since then, Don has worked on a number of fundamental problems in cosmochemistry, chronology of the solar system, the initial Pu/U abundance, fractionation of U and Pu in igneous processes, and elemental abundances. This last interest led him to advocate, propose, and lead the Genesis space mission to collect and return samples of the solar wind. The crash of the return capsule caused alarm, but some aspects of the mission were unaffected and others have been successfully handled, so that several major new results have been published: the lack of an SEP component in lunar samples, the Ne and Ar composition of the solar wind, and, most importantly, the oxygen and nitrogen isotopic composition of the Sun. Don received the Leonard Medal in 2012.
C1 NASA, Space Sci & Astrobiol Div, Bay Area Environm Res Inst, Ames Res Ctr, Mountain View, CA 94035 USA.
RP Sears, DWG (reprint author), NASA, Space Sci & Astrobiol Div, Bay Area Environm Res Inst, Ames Res Ctr, Mountain View, CA 94035 USA.
EM derek.sears@nasa.gov
FU NASA
FX This interview was recorded on February 5th, 2013, and edited by the
author and DB. I am grateful to NASA for financial support and to Tim
Jull and Hazel Sears for reviews and Hazel also for proofing.
NR 14
TC 0
Z9 0
U1 0
U2 2
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 SEP
PY 2013
VL 48
IS 9
BP 1715
EP 1732
DI 10.1111/maps.12180
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 264NQ
UT WOS:000327885300014
ER
PT J
AU Sears, DWG
AF Sears, Derek W. G.
TI Oral Histories in Meteoritics and Planetary Science-XXIII: Dieter
Stoffler
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID SHOCK METAMORPHISM; IMPACT; QUARTZ; CRATER
AB In this interview, Dieter Stoffler (Fig.1) describes how his interest in meteorites and impact craters dates from his Ph.D. studies at the University of Tubingen when it was learned that the Ries crater was formed by impact. A paper by Dieter's advisor, Wolf von Engelhardt, also triggered an interest in meteorites. After graduation, Dieter helped to establish a laboratory for high pressure mineralogy and he examined rocks from the Ries crater, which led to the concept of progressive shock metamorphism. The group also worked on newly returned Apollo samples and guided astronauts over the crater. A year at the NASA Ames Research Center taught Dieter about experimental impact research with a light-gas gun. After a few more years at Tubingen, Dieter obtained a professorship at the University of Munster where he created the Institute of Planetology, got involved in planning space missions including comet sample return, and continued high pressure mineralogy in collaboration with colleagues in Freiburg. Through several decades of research, Dieter and colleagues have documented the effects of shock on all the major rock-forming minerals and devised widely accepted schemes for the classification of shocked rocks. After the unification of Germany, Dieter became Director of the Natural History Museum in Berlin, during which he made much progress rebuilding the laboratories and the collections. Dieter also helped to create a museum and research center in the Ries crater. He received the Barringer Award of the Meteoritical Society in 1994 and several prestigious awards in Germany.
C1 NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Bay Area Environm Res Inst, Mountain View, CA 94035 USA.
RP Sears, DWG (reprint author), NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Bay Area Environm Res Inst, MS245-3, Mountain View, CA 94035 USA.
EM derek.sears@nasa.gov
FU NASA
FX This interview was recorded on April 3rd and 4th, 2013, and edited by
the author and DS. As of March 8th, 2013, a full CV and publication list
are posted online at:
http://mfnsu32.naturkundemuseumberlin.de/en/institution/mitarbeiter/stoe
ffler-dieter/. I am grateful to NASA for financial support and to
Natasha Artemieva, Tim Jull, and Hazel Sears for reviews and Hazel also
for proofing.
NR 22
TC 0
Z9 0
U1 0
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 SEP
PY 2013
VL 48
IS 9
BP 1733
EP 1751
DI 10.1111/maps.12179
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 264NQ
UT WOS:000327885300015
ER
PT J
AU Lagerloef, G
deCharon, A
Lindstrom, E
AF Lagerloef, Gary
deCharon, Annette
Lindstrom, Eric
TI Ocean Salinity and the Aquarius/SAC-D Mission: A New Frontier in Ocean
Remote Sensing
SO MARINE TECHNOLOGY SOCIETY JOURNAL
LA English
DT Editorial Material
ID DIELECTRIC-CONSTANT; SEA-WATER
C1 [Lagerloef, Gary] Earth & Space Res, Seattle, WA USA.
[deCharon, Annette] Univ Maine, Orono, ME 04469 USA.
[Lindstrom, Eric] NASA, Washington, DC 20546 USA.
RP Lagerloef, G (reprint author), Earth & Space Res, Seattle, WA USA.
NR 7
TC 6
Z9 6
U1 1
U2 10
PU MARINE TECHNOLOGY SOC INC
PI COLUMBIA
PA 5565 STERRETT PLACE, STE 108, COLUMBIA, MD 21044 USA
SN 0025-3324
EI 1948-1209
J9 MAR TECHNOL SOC J
JI Mar. Technol. Soc. J.
PD SEP-OCT
PY 2013
VL 47
IS 5
BP 26
EP 30
PG 5
WC Engineering, Ocean; Oceanography
SC Engineering; Oceanography
GA 256AC
UT WOS:000327281100004
ER
PT J
AU Monteleoni, C
Schmidt, GA
McQuade, S
AF Monteleoni, Claire
Schmidt, Gavin A.
McQuade, Scott
TI Climate Informatics: Accelerating Discovering in Climate Science with
Machine Learning
SO COMPUTING IN SCIENCE & ENGINEERING
LA English
DT Article
ID PREDICTION
AB The goal of climate informatics, an emerging discipline, is to inspire collaboration between climate scientists and data scientists, in order to develop tools to analyze complex and ever-growing amounts of observed and simulated climate data, and thereby bridge the gap between data and understanding. Here, recent climate informatics work is discussed, along with some of the field's remaining challenges.
C1 [Monteleoni, Claire; McQuade, Scott] George Washington Univ, Washington, DC 20052 USA.
[Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, Greenbelt, MD 20771 USA.
RP Monteleoni, C (reprint author), George Washington Univ, Washington, DC 20052 USA.
EM cmontel@gwu.edu; gavin.a.schmidt@nasa.gov; mcquade@gwmail.gwu.edu
RI Schmidt, Gavin/D-4427-2012
OI Schmidt, Gavin/0000-0002-2258-0486
NR 22
TC 3
Z9 3
U1 1
U2 5
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 1521-9615
EI 1558-366X
J9 COMPUT SCI ENG
JI Comput. Sci. Eng.
PD SEP-OCT
PY 2013
VL 15
IS 5
BP 32
EP 40
PG 9
WC Computer Science, Interdisciplinary Applications
SC Computer Science
GA 251AU
UT WOS:000326901000005
ER
PT J
AU Shen, BW
Nelson, B
Cheung, S
Tao, WK
AF Shen, Bo-Wen
Nelson, Bron
Cheung, Samson
Tao, Wei-Kuo
TI Improving NASA's Multiscale Modeling Framework for Tropical Cyclone
Climate Study
SO COMPUTING IN SCIENCE & ENGINEERING
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; WAVES
AB One of the current challenges in tropical cyclone research is how to improve our understanding of TCs' interannual variability as well as climate change's impact. Modern advances in global modeling, visualization, and supercomputing technologies at NASA show potential, but scalability is an issue. Recent improvements to the multiscale modeling framework make long-term TC-resolving simulations much more feasible.
C1 [Shen, Bo-Wen] Univ Maryland, College Pk, MD 20742 USA.
[Shen, Bo-Wen; Tao, Wei-Kuo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Shen, BW (reprint author), Univ Maryland, College Pk, MD 20742 USA.
EM bo-wen.shen-1@nasa.gov; bron.c.nelson@nasa.gov;
samson.h.cheung@nasa.gov; wei-kuo.tao-1@nasa.gov
FU NASA Earth Science Technology Office; Advanced Information Systems
Technology (AIST) Program; NASA Computational Modeling Algorithms and
Cyberinfrastructure (CMAC) program; NASA Modeling, Analysis Prediction
(MAP) Program; NASA High-End Computing (HEC) Program through the NASA
Advanced Supercomputing (NAS) Division at Ames Research Center
FX We're grateful to the following organizations for their support: the
NASA Earth Science Technology Office, the Advanced Information Systems
Technology (AIST) Program, the NASA Computational Modeling Algorithms
and Cyberinfrastructure (CMAC) program, and the NASA Modeling, Analysis
Prediction (MAP) Program. Resources supporting this work were provided
by the NASA High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center. Finally, we thank
Jill Dunbar of NASA ARC/NAS for proofreading this manuscript.
NR 20
TC 4
Z9 4
U1 0
U2 2
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 1521-9615
EI 1558-366X
J9 COMPUT SCI ENG
JI Comput. Sci. Eng.
PD SEP-OCT
PY 2013
VL 15
IS 5
BP 56
EP 67
PG 12
WC Computer Science, Interdisciplinary Applications
SC Computer Science
GA 251AU
UT WOS:000326901000007
ER
PT J
AU Rodrigues, BHG
Grindlay, JE
Allen, B
Hong, J
Barthelmy, S
Braga, J
D'Amico, F
Rothschild, RE
AF Rodrigues, B. H. G.
Grindlay, J. E.
Allen, B.
Hong, J.
Barthelmy, S.
Braga, J.
D'Amico, F.
Rothschild, R. E.
TI The high resolution X-ray imaging detector planes for the MIRAX mission
SO JOURNAL OF INSTRUMENTATION
LA English
DT Article
DE Gamma detectors (scintillators, CZT, HPG, HgI etc); X-ray detectors and
telescopes; Data analysis; Detector alignment and calibration methods
(lasers, sources, particle-beams)
AB The MIRAX X-ray observatory, the first Brazilian-led astrophysics space mission, is designed to perform an unprecedented wide-field, wide-band hard X-ray (5-200 keV) survey of Galactic X-ray transient sources. In the current configuration, MIRAX will carry a set of four coded-masks telescopes with high spatial resolution Cadmium Zinc Telluride (CZT) detector planes, each one consisting of an array of 64 closely tiled CZT pixelated detectors. Taken together, the four telescopes will have a total detection area of 959 cm(2), a large field of view (60 degrees x 60 degrees FWHM), high angular resolution for this energy range (6 arcmin) and very good spectral resolution (similar to 2 keV @ 60 keV). A stratospheric balloon-borne prototype of one of the MIRAX telescopes has been developed, tested and flown by the Harvard-Smithsonian Center for Astrophysics (CfA) as part of the ProtoEXIST program. In this paper we show results of validation and calibration tests with individual CZT detectors of the ProtoEXIST second generation experiment (P2). Each one of 64 detector units of the P2 detector plane consists of an ASIC, developed by Caltech for the NuSTAR telescope, hybridized to a CZT crystal with 0.6mm pixel size. The performance of each detector was evaluated using radioactive sources in the laboratory. The calibration results show that the P2 detectors have average energy resolution of similar to 2.1 keV @ 60 keV and 2.3 @ 122 keV. P2 was also successfully tested on near-space environment on a balloon flight, demonstrating the detector unit readiness for integration on a space mission telescope, as well as satisfying all MIRAX mission requirements.
C1 [Rodrigues, B. H. G.; Braga, J.; D'Amico, F.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Rodrigues, B. H. G.; Grindlay, J. E.; Allen, B.; Hong, J.] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA.
[Barthelmy, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rothschild, R. E.] Univ Calif San Diego, La Jolla, CA 92093 USA.
RP Rodrigues, BHG (reprint author), Inst Nacl Pesquisas Espaciais, Av Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
EM barbara@das.inpe.br
FU NASA [NNX09AD76G, NNX11AF35G]; CAPES
FX We would like to thank MIRAX and ProtoEXIST technical teams for the
great effort done for this mission development. Special thanks to J.
Grindlay and CAPES for fellowship grants. Development of the ProtoEXIST
program and P2 detector and telescope at Harvard is currently supported
by NASA grants NNX09AD76G and NNX11AF35G.
NR 15
TC 1
Z9 1
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-0221
J9 J INSTRUM
JI J. Instrum.
PD SEP
PY 2013
VL 8
AR P09010
DI 10.1088/1748-0221/8/09/P09010
PG 14
WC Instruments & Instrumentation
SC Instruments & Instrumentation
GA 248FL
UT WOS:000326680200024
ER
PT J
AU Helmboldt, JF
Clarke, TE
Craig, J
Dowell, JD
Ellingson, SW
Hartman, JM
Hicks, BC
Kassim, NE
Taylor, GB
Wolfe, CN
AF Helmboldt, J. F.
Clarke, T. E.
Craig, J.
Dowell, J. D.
Ellingson, S. W.
Hartman, J. M.
Hicks, B. C.
Kassim, N. E.
Taylor, G. B.
Wolfe, C. N.
TI Passive all-sky imaging radar in the HF regime with WWV and the first
station of the Long Wavelength Array
SO RADIO SCIENCE
LA English
DT Article
DE HF radar; ionospheric tilts; sporadic-E; HF terrain mapping
ID BISTATIC RADAR; SYSTEMS
AB We present a new passive, bistatic high-frequency (HF) radar system consisting of the transmitters for the radio station WWV and the dipole antenna array that comprises the first station of the Long Wavelength Array (LWA) or LWA1. We demonstrate that these two existing facilities, which are operated for separate purposes, can be used together as a unique HF radar imager, capable of monitoring the entire visible sky. In this paper, we describe in detail the techniques used to develop all-sky radar capability at 10, 15, and 20 MHz. We show that this radar system can be a useful tool for probing ionospheric structure and its effect on over-the-horizon (OTH) geolocation. The LWA1+WWV radar system appears to be especially adept at detecting and characterizing structures associated with sporadic-E. In addition, we also demonstrate how this system may be used for long-distance, OTH mapping of terrain/ocean HF reflectivity. Finally, we discuss the potential improvements in the utility of these applications as more LWA stations are added.
C1 [Helmboldt, J. F.; Clarke, T. E.; Hicks, B. C.; Kassim, N. E.] US Naval Res Lab, Washington, DC 20375 USA.
[Craig, J.; Dowell, J. D.; Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
[Ellingson, S. W.; Wolfe, C. N.] Virginia Tech, Bradley Dept Elect & Comp Engn, Blacksburg, VA USA.
[Hartman, J. M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Taylor, G. B.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP Helmboldt, JF (reprint author), US Naval Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA.
EM joe.helmboldt@nrl.navy.mil
RI Helmboldt, Joseph/C-8105-2012
FU NASA Postdoctoral Program at the Jet Propulsion Laboratory; NASA; Naval
Research Laboratory; Office of Naval Research [N00014-07-C=0147];
National Science Foundation of the University Radio Observatory program
[AST-1139974]; National Aeronautics and Space Administration
FX This research was supported by an appointment to the NASA Postdoctoral
Program at the Jet Propulsion Laboratory, administered by Oak Ridge
Universities through a contract with NASA. The authors would like to
thank F. Schinzel and T. Pedersen for useful comments and suggestions.
Basic research in astronomy at the Naval Research Laboratory is
supported by 6.1 base funding. Construction of the LWA has been
supported by the Office of Naval Research under contract
N00014-07-C=0147. Support for operations and continuing development of
the LWA1 is provided by the National Science Foundation under grant
AST-1139974 of the University Radio Observatory program. 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 29
TC 3
Z9 3
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
EI 1944-799X
J9 RADIO SCI
JI Radio Sci.
PD SEP
PY 2013
VL 48
IS 5
BP 491
EP 512
DI 10.1002/rds.20056
PG 22
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA 252RW
UT WOS:000327028500003
ER
PT J
AU Crucian, B
Quiriarte, H
Guess, T
Ploutz-Snyder, R
McMonigal, K
Sams, C
AF Crucian, Brian
Quiriarte, Heather
Guess, Terry
Ploutz-Snyder, Robert
McMonigal, Kathleen
Sams, Clarence
TI A Miniaturized Analyzer Capable of White-Blood-Cell and Differential
Analyses During Spaceflight
SO LABMEDICINE
LA English
DT Article
DE spaceflight; hematology analyzer
ID GRAVITY
AB Spaceflight has adverse effects on the human body that pose health risks to astronauts spending extended time in space missions. For clinical monitoring of astronauts and for in-flight biomedical research, laboratory instruments must be available in the spaceflight environment. Currently, no instrument has been shown to be capable of generating a white blood cell (WBC) count and differential during spaceflight to our knowledge, although this is a medical requirement of the National Aeronautics and Space Administration (NASA). We evaluated a compact hematology analyzer for compatibility with a zero-gravity environment. We performed analyses in reduced-gravity during parabolic flight. Herein, we describe our engineering evaluation and report the reduced-gravity validation data we collected. The hematology analyzer we tested met the basic requirements for use in spaceflight and should be capable of accurately measuring WBC parameters aboard the International Space Station.
C1 [Crucian, Brian; McMonigal, Kathleen; Sams, Clarence] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Quiriarte, Heather] JES Tech LLC, Houston, TX USA.
[Guess, Terry] Wyle Sci Technol & Engn, Houston, TX USA.
[Ploutz-Snyder, Robert] Univ Space Res Assoc, Houston, TX USA.
RP Crucian, B (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM brian.crucian-1@nasa.gov
FU NASA-Johnson Space Center (JSC) Internal Research and Development (IRD)
Program
FX The authors thank the NASA-Johnson Space Center (JSC) Internal Research
and Development (IR&D) Program for funding this study, the JSC Clinical
Laboratory for providing control data, and the JSC Reduced Gravity
Office for facilitating the parabolic-flight opportunity.
NR 14
TC 4
Z9 4
U1 0
U2 4
PU AMER SOC CLINICAL PATHOLOGY
PI CHICAGO
PA 2100 W HARRISON ST, CHICAGO, IL 60612 USA
SN 0007-5027
EI 1943-7730
J9 LABMEDICINE
JI Labmedicine
PD FAL
PY 2013
VL 44
IS 4
BP 304
EP 312
DI 10.1309/LMD3THAYCHICF2XT
PG 9
WC Medical Laboratory Technology
SC Medical Laboratory Technology
GA 238AF
UT WOS:000325912100003
ER
PT J
AU Turpie, KR
AF Turpie, Kevin R.
TI Explaining the Spectral Red-Edge Features of Inundated Marsh Vegetation
SO JOURNAL OF COASTAL RESEARCH
LA English
DT Article
DE Tidal marsh; canopy reflectance spectra; water reflectance spectra;
spectral reflectance modeling; red-edge position; coastal vegetation
remote sensing
ID CANOPY REFLECTANCE MODEL; CHLOROPHYLL CONTENT; LEAF CHLOROPHYLL; SHALLOW
WATERS; PLANT CANOPY; POSITION; SPECTROMETRY; INVERSION; INDEX; SHAPE
AB In a previously published experiment, canopy reflectance spectrum was measured for three monospecific canopies as water level was artificially increased. As the water rose, spectral features appeared that could not be explained by the experimenters. To better understand their published results, a combination of a shallow-water reflectance model and a canopy reflectance model was used to simulate the spectral effects observed with increasing levels of inundation. Information from the Lee shallow water, in particular, helped explain the key spectral features observed during high water levels. However, the simulation results also suggested interesting implications regarding the nonlinear mixing of water and vegetation reflection spectra as found in marsh or other flooded canopies. As water level increases, the influence of leaf reflectance below the water's surface changes the characteristics of the background aquatic spectrum. In particular, the simulation yielded a 20-nm shift in the red-edge position as water rose from the bottom to the top of the canopy, which is very similar to the experimental results. This suggests that the interaction of water and chlorophyll absorption features and leaf reflectance near the red-edge of the vegetation spectrum can significantly the influence red-edge position of an inundated canopy. This, in turn, could affect the use of the red-edge position for indicating plant condition in remote-sensing applications of inundated vegetation.
C1 NASA, Goddard Space Flight Ctr, Ocean Ecol Branch, Greenbelt, MD 20771 USA.
RP Turpie, KR (reprint author), NASA, Goddard Space Flight Ctr, Ocean Ecol Branch, Code 616-2, Greenbelt, MD 20771 USA.
EM kturpie@umbc.edu
NR 36
TC 7
Z9 7
U1 2
U2 9
PU COASTAL EDUCATION & RESEARCH FOUNDATION
PI LAWRENCE
PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA
SN 0749-0208
EI 1551-5036
J9 J COASTAL RES
JI J. Coast. Res.
PD SEP
PY 2013
VL 29
IS 5
BP 1111
EP 1117
DI 10.2112/JCOASTRES-D-12-00209.1
PG 7
WC Environmental Sciences; Geography, Physical; Geosciences,
Multidisciplinary
SC Environmental Sciences & Ecology; Physical Geography; Geology
GA 243GL
UT WOS:000326304800013
ER
PT J
AU Diniega, S
Smrekar, SE
Anderson, S
Stofan, ER
AF Diniega, S.
Smrekar, S. E.
Anderson, S.
Stofan, E. R.
TI The influence of temperature-dependent viscosity on lava flow dynamics
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
DE lava; flow dynamics; instabilities; viscous fingering; sheet flow
ID KILAUEA VOLCANO; MOUNT-ETNA; MAUNA-ULU; PAHOEHOE LAVA;
SURFACE-MORPHOLOGY; FISSURE ERUPTIONS; MAGMA FLOW; HAWAII; EMPLACEMENT;
CRYSTALLIZATION
AB Many studies have investigated how channels and tubes form within basaltic flows. The partitioning of a broad lava flow into narrow regions of enhanced flow velocity (which we refer to as preferred pathways) can affect lava emplacement, and allow flows to reach great lengths on Earth and other planets. In this study, we investigate the role that a dynamic instability, driven by large changes in viscosity due to small changes in temperature, can play in the formation and propagation of low-viscosity preferred pathways. We use a fluid dynamics-based model of laminar lava flow emplacement that examines this process exclusively. Analysis of this model shows that preferred pathways will initiate when the temperature dependence of the lava's viscosity is sufficiently strong. If a preferred pathway develops, it will form and stabilize over a distance that reflects the competition between the cooling rate through the flow's surfaces and the flow velocity within the preferred pathway. Using velocity and cooling rates of typical basaltic flows on Earth, this model is able to produce preferred pathways within lava flows with reasonable dimensions and timescales. The model also fails to produce such pathways in situations where tubes and channels are not found in nature (e.g., in basalt sheet flows and silicic flows<1km in length). These results are sufficiently positive to demonstrate that this thermodynamic instability may play a role in the formation and propagation of preferred pathways within some flows, and thus merit further investigation.
C1 [Diniega, S.; Smrekar, S. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Anderson, S.] Univ No Colorado, MAST Inst, Greeley, CO 80639 USA.
[Anderson, S.] Univ No Colorado, Dept Earth Sci, Greeley, CO 80639 USA.
[Stofan, E. R.] Proxemy Res, Rectortown, VA USA.
RP Diniega, S (reprint author), CALTECH, Jet Prop Lab, M-S 301-250D,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM serina.diniega@jpl.nasa.gov
FU NASA [NNG05GL55G]
FX Diniega was supported by an appointment to the NASA Postdoctoral
Program, administered by Oak Ridge Associated Universities, at the
California Institute of Technology Jet Propulsion Laboratory under a
contract with NASA. Anderson acknowledges support from grant NNG05GL55G
from the NASA Mars Fundamental Research Program. We thank two reviewers
and two editors for their extensive comments which have greatly improved
the manuscript. We also thank Christophe Sotin for suggesting the
flux-limiting method.
NR 86
TC 0
Z9 0
U1 1
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9003
EI 2169-9011
J9 J GEOPHYS RES-EARTH
JI J. Geophys. Res.-Earth Surf.
PD SEP
PY 2013
VL 118
IS 3
BP 1516
EP 1532
DI 10.1002/jgrf.20111
PG 17
WC Geosciences, Multidisciplinary
SC Geology
GA 238VC
UT WOS:000325978500023
ER
PT J
AU Morlighem, M
Seroussi, H
Larour, E
Rignot, E
AF Morlighem, M.
Seroussi, H.
Larour, E.
Rignot, E.
TI Inversion of basal friction in Antarctica using exact and incomplete
adjoints of a higher-order model
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
DE inverse method; exact adjoint; incomplete adjoint; basal friction;
large-scale modeling
ID ICE-SHEET MODEL; SATELLITE RADAR; FLOW MODEL; GLACIERS; THICKNESS; SHELF
AB Basal friction beneath ice sheets remains poorly characterized and yet is a fundamental control on ice mechanics. Here we use a complete map of surface velocity of the Antarctic Ice Sheet to infer the basal friction over the entire continent by combining these observations with a three-dimensional, thermomechanical, higher-order ice sheet numerical model from the Ice Sheet System Model open source software. We demonstrate that inverse methods can be readily applied at the continental scale with appropriate selections of cost function and of scheme of regularization, at a spatial resolution as high as 3 km along the coastline. We compare the convergence of two descent algorithms with the exact and incomplete adjoints to show that the incomplete adjoint is an excellent approximation. The results reveal that the driving stress is almost entirely balanced by the basal shear stress over 80% of the ice sheet. The basal friction coefficient, which relates basal friction to basal velocity, is, however, significantly heterogeneous: it is low on fast moving ice and high near topographic divides. Areas with low values extend far out into the interior, along glacier and ice stream tributaries, almost to the flanks of topographic divides, suggesting that basal sliding is widespread beneath the Antarctic Ice Sheet.
C1 [Morlighem, M.; Rignot, E.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Seroussi, H.; Larour, E.; Rignot, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Morlighem, M (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Croul Hall, Irvine, CA 92697 USA.
EM Mathieu.Morlighem@uci.edu
RI Rignot, Eric/A-4560-2014; Morlighem, Mathieu/O-9942-2014
OI Rignot, Eric/0000-0002-3366-0481; Morlighem, Mathieu/0000-0001-5219-1310
FU National Aeronautics and Space Administration, Cryospheric Sciences
Program [NNX12AB86G]; NASA
FX This work was performed at the Department of Earth System Science,
University of California, Irvine and at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration, Cryospheric Sciences Program,
grant NNX12AB86G. Helene Seroussi 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. We
thank the two anonymous reviewers, the Associate Editor J. Bassis, and
the Editor B. Hubbard for their helpful and insightful comments.
NR 34
TC 28
Z9 28
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9003
EI 2169-9011
J9 J GEOPHYS RES-EARTH
JI J. Geophys. Res.-Earth Surf.
PD SEP
PY 2013
VL 118
IS 3
BP 1746
EP 1753
DI 10.1002/jgrf.20125
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA 238VC
UT WOS:000325978500038
ER
PT J
AU Asseng, S
Ewert, F
Rosenzweig, C
Jones, JW
Hatfield, JL
Ruane, AC
Boote, KJ
Thorburn, PJ
Rotter, RP
Cammarano, D
Brisson, N
Basso, B
Martre, P
Aggarwal, PK
Angulo, C
Bertuzzi, P
Biernath, C
Challinor, AJ
Doltra, J
Gayler, S
Goldberg, R
Grant, R
Heng, L
Hooker, J
Hunt, LA
Ingwersen, J
Izaurralde, RC
Kersebaum, KC
Muller, C
Kumar, SN
Nendel, C
O'Leary, G
Olesen, JE
Osborne, TM
Palosuo, T
Priesack, E
Ripoche, D
Semenov, MA
Shcherbak, I
Steduto, P
Stockle, C
Stratonovitch, P
Streck, T
Supit, I
Tao, F
Travasso, M
Waha, K
Wallach, D
White, JW
Williams, JR
Wolf, J
AF Asseng, S.
Ewert, F.
Rosenzweig, C.
Jones, J. W.
Hatfield, J. L.
Ruane, A. C.
Boote, K. J.
Thorburn, P. J.
Rotter, R. P.
Cammarano, D.
Brisson, N.
Basso, B.
Martre, P.
Aggarwal, P. K.
Angulo, C.
Bertuzzi, P.
Biernath, C.
Challinor, A. J.
Doltra, J.
Gayler, S.
Goldberg, R.
Grant, R.
Heng, L.
Hooker, J.
Hunt, L. A.
Ingwersen, J.
Izaurralde, R. C.
Kersebaum, K. C.
Mueller, C.
Kumar, S. Naresh
Nendel, C.
O'Leary, G.
Olesen, J. E.
Osborne, T. M.
Palosuo, T.
Priesack, E.
Ripoche, D.
Semenov, M. A.
Shcherbak, I.
Steduto, P.
Stoeckle, C.
Stratonovitch, P.
Streck, T.
Supit, I.
Tao, F.
Travasso, M.
Waha, K.
Wallach, D.
White, J. W.
Williams, J. R.
Wolf, J.
TI Uncertainty in simulating wheat yields under climate change
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID CROP PRODUCTION; MODELS; FOOD; CO2; TEMPERATURE; PROJECTIONS;
ADAPTATION; SCENARIOS; ENSEMBLE; IMPACTS
AB Projections of climate change impacts on crop yields are inherently uncertain(1). Uncertainty is often quantified when projecting future greenhouse gas emissions and their influence on climate(2). However, multi-model uncertainty analysis of crop responses to climate change is rare because systematic and objective comparisons among process-based crop simulation models(1,3) are difficult(4). Here we present the largest standardized model intercomparison for climate change impacts so far. We found that individual crop models are able to simulate measured wheat grain yields accurately under a range of environments, particularly if the input information is sufficient. However, simulated climate change impacts vary across models owing to differences in model structures and parameter values. A greater proportion of the uncertainty in climate change impact projections was due to variations among crop models than to variations among downscaled general circulation models. Uncertainties in simulated impacts increased with CO2 concentrations and associated warming. These impact uncertainties can be reduced by improving temperature and CO2 relationships in models and better quantified through use of multi-model ensembles. Less uncertainty in describing how climate change may affect agricultural productivity will aid adaptation strategy development and policymaking.
C1 [Asseng, S.; Jones, J. W.; Cammarano, D.] Univ Florida, Dept Agr & Biol Engn, Gainesville, FL 32611 USA.
[Ewert, F.; Angulo, C.] Univ Bonn, Inst Crop Sci & Resource Conservat INRES, D-53115 Bonn, Germany.
[Rosenzweig, C.; Ruane, A. C.; Goldberg, R.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Hatfield, J. L.] Natl Lab Agr & Environm, Ames, IA 50011 USA.
[Boote, K. J.] Univ Florida, Dept Agron, Gainesville, FL 32611 USA.
[Thorburn, P. J.] CSIRO Ecosyst Sci, Dutton Pk, Qld 4102, Australia.
[Rotter, R. P.; Palosuo, T.] MTT Agrifood Res Finland, Plant Prod Res, FI-50100 Mikkeli, Finland.
[Brisson, N.] INRA, Agron UMR0211, F-78750 Thiverval Grignon, France.
[Brisson, N.] AgroParisTech, Agron UMR0211, F-78750 Thiverval Grignon, France.
[Basso, B.; Shcherbak, I.] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48823 USA.
[Basso, B.; Shcherbak, I.] Michigan State Univ, WK Kellogg Biol Stn, E Lansing, MI 48823 USA.
[Martre, P.] INRA, GDEC UMR1095, F-63100 Clermont Ferrand, France.
[Martre, P.] Univ Blaise Pascal, UMR1095 GDEC, F-63170 Clermont Ferrand, France.
[Aggarwal, P. K.] IWMI, CCAFS, New Delhi 12, India.
[Bertuzzi, P.; Ripoche, D.] INRA, AgroClim US1116, F-84914 Avignon, France.
[Biernath, C.; Priesack, E.] German Res Ctr Environm Hlth, Helmholtz Zentrum Munchen, Inst Soil Ecol, D-85764 Neuherberg, Germany.
[Challinor, A. J.] Univ Leeds, Sch Earth & Environm, Inst Climate & Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England.
[Challinor, A. J.] CIAT, CGIAR ESSP Program Climate Change Agr & Food Secu, Cali 6713, Colombia.
[Doltra, J.] Cantabrian Agr Res & Training Ctr CIFA, Muriedas 39600, Spain.
[Gayler, S.] Univ Tubingen, WESS Water & Earth Syst Sci Competence Cluster, D-72074 Tubingen, Germany.
[Grant, R.] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2E3, Canada.
[Heng, L.] IAEA, A-1400 Vienna, Austria.
[Hooker, J.] Univ Reading, Dept Agr, Reading RG6 6AR, Berks, England.
[Hunt, L. A.] Univ Guelph, Dept Plant Agr, Guelph, ON N1G 2W1, Canada.
[Ingwersen, J.; Streck, T.] Univ Hohenheim, Inst Soil Sci & Land Evaluat, D-70593 Stuttgart, Germany.
[Izaurralde, R. C.] Joint Global Change Res Inst, College Pk, MD 20740 USA.
[Kersebaum, K. C.; Nendel, C.] Leibniz Ctr Agr Landscape Res, Inst Landscape Syst Anal, D-15374 Muncheberg, Germany.
[Mueller, C.; Waha, K.] Potsdam Inst Climate Impact Res, D-14473 Potsdam, Germany.
[Kumar, S. Naresh] IARI PUSA, Indian Agr Res Inst, Ctr Environm Sci & Climate Resilient Agr, New Delhi 110012, India.
[O'Leary, G.] Dept Primary Ind, Horsham, Vic 3400, Australia.
[Olesen, J. E.] Aarhus Univ, Dept Agroecol, DK-8830 Tjele, Denmark.
[Osborne, T. M.] Univ Reading, Walker Inst, NCAS Climate, Reading RG6 6BB, Berks, England.
[Semenov, M. A.; Stratonovitch, P.] Rothamsted Res, Computat & Syst Biol Dept, Harpenden AL5 2JQ, Herts, England.
[Steduto, P.] FAO, I-00100 Rome, Italy.
[Stoeckle, C.] Washington State Univ, Pullman, WA 99164 USA.
[Supit, I.; Wolf, J.] Wageningen Univ, NL-6700 AA Wageningen, Netherlands.
[Tao, F.] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Beijing 100101, Peoples R China.
[Travasso, M.] INTA CIRN, Inst Climate & Water, RA-1712 Castelar, Argentina.
[Wallach, D.] INRA, UMR Agrosyst & Dev Terr AGIR 1248, F-31326 Castanet Tolosan, France.
[White, J. W.] Arid Land Agr Res Ctr, Maricopa, AZ 85138 USA.
[Williams, J. R.] Texas A&M Univ, Temple, TX 76502 USA.
RP Asseng, S (reprint author), Univ Florida, Dept Agr & Biol Engn, Gainesville, FL 32611 USA.
RI Thorburn, Peter/A-6884-2011; Martre, Pierre/M-5282-2013; Palosuo,
Taru/B-9593-2012; Priesack, Eckart/M-7341-2014; Nendel,
Claas/C-8844-2013; Challinor, Andrew/C-4992-2008; Doltra,
Jordi/C-2106-2015; Basso, Bruno/A-3128-2012; Martre, Pierre/G-5399-2013;
Mueller, Christoph/E-4812-2016; Olesen, Jorgen/C-2905-2016;
OI Boote, Kenneth/0000-0002-1358-5496; Kersebaum, Kurt
Christian/0000-0002-3679-8427; Priesack, Eckart/0000-0002-5088-9528;
Stratonovitch, Pierre/0000-0002-5806-2066; Cammarano,
Davide/0000-0003-0918-550X; Wallach, Daniel/0000-0003-3500-8179; Martre,
Pierre/0000-0002-7419-6558; Palosuo, Taru/0000-0003-4322-3450; Nendel,
Claas/0000-0001-7608-9097; Challinor, Andrew/0000-0002-8551-6617; Basso,
Bruno/0000-0003-2090-4616; Martre, Pierre/0000-0002-7419-6558; Mueller,
Christoph/0000-0002-9491-3550; Olesen, Jorgen/0000-0002-6639-1273;
Grant, Robert/0000-0002-8890-6231
NR 30
TC 251
Z9 254
U1 37
U2 267
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 SEP
PY 2013
VL 3
IS 9
BP 827
EP 832
DI 10.1038/NCLIMATE1916
PG 6
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 249YD
UT WOS:000326816100022
ER
PT J
AU Pau, S
Wolkovich, EM
Cook, BI
Nytch, CJ
Regetz, J
Zimmerman, JK
Wright, SJ
AF Pau, Stephanie
Wolkovich, Elizabeth M.
Cook, Benjamin I.
Nytch, Christopher J.
Regetz, James
Zimmerman, Jess K.
Wright, S. Joseph
TI Clouds and temperature drive dynamic changes in tropical flower
production
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID RAIN-FOREST TREE; AMAZON FOREST; DROUGHT; GROWTH; CLIMATE; PLANTS
AB Tropical forests are incredibly dynamic, showing rapid and longer-term changes in growth, mortality and net primary productivity(1-3). Tropical species may be highly sensitive to temperature increases associated with climate change because of their narrow thermal tolerances. However, at the ecosystem scale the competing effects of temperature, light and precipitation on tropical forest productivity have been difficult to assess. Here we quantify cloudiness over the past several decades to investigate how clouds, together with temperature and precipitation, affect flower production in two contrasting tropical forests. Our results show that temperature, rather than clouds, is critically important to tropical forest flower production. Warmer temperatures increased flower production over seasonal, interannual and longer timescales, contrary to recent evidence that some tropical forests are already near their temperature threshold(4,5). Clouds were primarily important seasonally, and limited production in a seasonally dry forest but enhanced production in an ever-wet forest. A long-term increase in flower production at the seasonally dry forest is not driven by clouds and instead may be tied to increasing temperatures. These relationships show that tropical forest productivity, which is not widely thought to be controlled by temperature, is indeed sensitive to small temperature changes (1-4 degrees C) across multiple timescales.
C1 [Pau, Stephanie] Florida State Univ, Dept Geog, Tallahassee, FL 32306 USA.
[Pau, Stephanie; Regetz, James] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA.
[Wolkovich, Elizabeth M.] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada.
[Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Cook, Benjamin I.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Nytch, Christopher J.; Zimmerman, Jess K.] Univ Puerto Rico, Inst Trop Ecosyst Studies, Rio Piedras, PR 00931 USA.
[Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama.
RP Pau, S (reprint author), Florida State Univ, Dept Geog, Tallahassee, FL 32306 USA.
EM spau@fsu.edu
RI Cook, Benjamin/H-2265-2012; Wright, Stuart/M-3311-2013
OI Wright, Stuart/0000-0003-4260-5676
FU National Center for Ecological Analysis and Synthesis (NCEAS); NSF
[EF-0553768, DEB-0639393, BSR-8811902, DEB-9411973, DEB-008538,
DEB-0218039, DEB-0620910]; University of California, Santa Barbara;
State of California; Environmental Sciences Program; Center for Tropical
Forest Science of the Smithsonian Institution; NCEAS; NSERC CREATE
training programme in biodiversity research
FX We thank K. Knapp at NOAA NCDC for providing a beta version of the full
GridSat data set, and D. K. Okamoto for input on statistical analyses,
and are also grateful to H.G.B. This work was conducted as a part of the
Forecasting Phenology Working Group supported by the National Center for
Ecological Analysis and Synthesis (NCEAS), a Center funded by the NSF
(Grant #EF-0553768), the University of California, Santa Barbara, and
the State of California. The BCI portion of the study was supported by
funds from the Environmental Sciences Program and the Center for
Tropical Forest Science of the Smithsonian Institution. At Luquillo
research was supported by NSF grant DEB-0639393 and by NSF funds
(BSR-8811902, DEB-9411973, DEB-008538, DEB-0218039 and DEB-0620910) to
the Luquillo Long-Term Ecological Research Program. S.P. was a
Postdoctoral Associate supported by NCEAS. E.M.W. was supported by the
NSERC CREATE training programme in biodiversity research.
NR 30
TC 15
Z9 15
U1 7
U2 37
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 SEP
PY 2013
VL 3
IS 9
BP 838
EP 842
DI 10.1038/NCLIMATE1934
PG 5
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 249YD
UT WOS:000326816100024
ER
PT J
AU Hong, XD
Wang, SP
Holt, TR
Martin, PJ
O'Neill, L
AF Hong, Xiaodong
Wang, Shouping
Holt, Teddy R.
Martin, Paul J.
O'Neill, Larry
TI Modulation of the sea-surface temperature in the Southeast Pacific by
the atmospheric low-level coastal jet
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE Ekman pumping; Ekman transport; surface heat flux; two-way coupled
air-ocean model; low-level coastal jet; satellite observation
ID EKMAN TRANSPORT; BOUNDARY-LAYER; WEST-COAST; VOCALS-REX; EL-NINO; MODEL;
VARIABILITY; OCEAN; MESOSCALE; DYNAMICS
AB The atmospheric low-level coastal jet (LLCJ) in the Southeast Pacific (SEP) region is characterized as either a strong-forcing jet (colder and drier air) or weak-forcing jet (warm and moist) based on the location of the Southeast Pacific high-pressure system (SEPH). The sea-surface temperature (SST) changes corresponding to a particularly strong-forcing jet (29-30 October) and weak-forcing jet (22-23 November) are investigated in this study using the two-way air-ocean coupled model COAMPS (R) and satellite observation data. Results indicate that the coupled simulation reduces the overall absolute bias 50% for the surface wind speed, 70% for the cloud liquid water path, and 15% for SST as compared to the uncoupled simulation. The coupled simulation reduces excessive SST cooling, especially during the strong-forcing jet period along the coastal area where offshore transport of upwelled cold water is too strong from the uncoupled simulation. The coupled simulation also reduces the excessive warming from the uncoupled simulation by providing better cloud coverage. The prominent mechanisms in cooling SST along the coast are the same for both the strong-forcing and weak-forcing jets, namely vigorous upwelling and horizontal advection. However, the mechanisms along the jet path differ from along the coast, with air-sea heat exchange the most important process, resulting in cooling SST during the strong-forcing jet period but warming SST during the weak-forcing jet period. The advances and differences of the present study as compared with previous studies are discussed in detail in the paper.
C1 [Hong, Xiaodong; Wang, Shouping; Holt, Teddy R.] Naval Res Lab, Monterey, CA 93943 USA.
[Martin, Paul J.] Naval Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS USA.
[O'Neill, Larry] Oregon State Univ, Coll Earth & Atmospher Sci, Corvallis, OR 97331 USA.
RP Hong, XD (reprint author), Naval Res Lab, 7 Grace Hopper Ave, Monterey, CA 93943 USA.
EM hong@nrlmry.navy.mil
FU NRL Base Program [PE 0602435N]
FX We would like to thank the reviewers for their constructive and many
helpful suggestions for improving this paper. This research is supported
by the NRL Base Program, PE 0602435N. Computations were performed on the
IBM P4+ at the Naval Oceanographic Office (NAVO) Major Shared Resource
Center (MSRC) at Stennis Space Center, Mississippi.
NR 44
TC 0
Z9 0
U1 0
U2 10
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 SEP
PY 2013
VL 118
IS 9
BP 3979
EP 3998
DI 10.1002/jgrc.20289
PG 20
WC Oceanography
SC Oceanography
GA 242HQ
UT WOS:000326230200001
ER
PT J
AU Jacobs, S
Giulivi, C
Dutrieux, P
Rignot, E
Nitsche, F
Mouginot, J
AF Jacobs, S.
Giulivi, C.
Dutrieux, P.
Rignot, E.
Nitsche, F.
Mouginot, J.
TI Getz Ice Shelf melting response to changes in ocean forcing
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE Antarctic; Amundsen; meltwater; thermocline; ice; shelf
ID CIRCUMPOLAR DEEP-WATER; PINE ISLAND GLACIER; CENTRAL AMUNDSEN SHELF;
SEA-ICE; ANTARCTIC PENINSULA; WEST ANTARCTICA; SHEET; TRANSPORT;
VARIABILITY; CIRCULATION
AB The large and complex Getz Ice Shelf extends along nearly half of the West Antarctic coastline in the Amundsen Sea and is exposed to a more variable ocean environment than most other Pacific sector ice shelves. Ocean temperature, salinity, and dissolved oxygen profiles acquired near its sub-ice cavity openings are used here to estimate seawater transports and meltwater fractions. More complete coverage during 2000 and 2007 brackets most of the variability observed from 1994 to 2011, and yearlong records near one ice front support the use of summer profiles to determine annual basal melt rates. We find area average rates of 1.1 and 4.1 m/yr, higher in 2007 when a larger volume of warmer deep water occupied the adjacent continental shelf, and the ocean circulation was stronger. Results are consistent with changes in thermocline depths relative to ice shelf draft and mass transports onto the adjacent continental shelf. We also calculate steady state and actual melting of 2.5 and 4.6 m/yr in 2007-2008 from satellite measurements of ice flux, modeled accumulation, and thinning from 2003 to 2008. This implies a positive mass balance in 2000, but negative in 2007, when the Getz was producing more meltwater than any of the larger, slower melting or smaller, faster-melting ice shelves.
C1 [Jacobs, S.; Giulivi, C.; Nitsche, F.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Dutrieux, P.] British Antarctic Survey, NERC, Cambridge CB3 0ET, England.
[Rignot, E.; Mouginot, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Rignot, E.; Mouginot, J.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
RP Jacobs, S (reprint author), Lamont Doherty Earth Observ, 205 Oceanog,Route 9W, Palisades, NY 10964 USA.
EM sjacobs@ldeo.columbia.edu
RI Rignot, Eric/A-4560-2014; Mouginot, Jeremie/G-7045-2015; Dutrieux,
Pierre/B-7568-2012;
OI Rignot, Eric/0000-0002-3366-0481; Dutrieux, Pierre/0000-0002-8066-934X;
Nitsche, Frank Oliver/0000-0002-4137-547X
FU NSF [ANT-0632282, ANT-0440775, OPP-9725024]; NOAA [NA08OAR4320912]; NERC
[NE/G001367/1]; NASA [NNX08AN28A, NNX10AV16G]; Lamont-Doherty Earth
Observatory [7717]
FX We thank the many individuals who have assisted with data acquisition
and processing, R. Guerrero, D. Shoosmith, and S. Stammerjohn for CTD
observations from other ships and NB Palmer cruises, and reviewers for
constructive comments. This work was supported by NSF grants
ANT-0632282, ANT-0440775, and OPP-9725024, and NOAA award NA08OAR4320912
to Columbia University, NERC grant NE/G001367/1 to the British Antarctic
Survey, NASA grants NNX08AN28A and NNX10AV16G to the University of
California, Irvine, and by the Lamont-Doherty Earth Observatory,
contribution 7717.
NR 47
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Z9 19
U1 0
U2 23
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 SEP
PY 2013
VL 118
IS 9
BP 4152
EP 4168
DI 10.1002/jgrc.20298
PG 17
WC Oceanography
SC Oceanography
GA 242HQ
UT WOS:000326230200011
ER
PT J
AU Dushaw, BD
Worcester, PF
Dzieciuch, MA
Menemenlis, D
AF Dushaw, B. D.
Worcester, P. F.
Dzieciuch, M. A.
Menemenlis, D.
TI On the time-mean state of ocean models and the properties of long range
acoustic propagation
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE acoustic thermometry; ocean models; model testing
ID NORTH PACIFIC-OCEAN; SOUND-PROPAGATION; INTERNAL TIDES; KAUAI SOURCE;
TRANSMISSIONS; TOMOGRAPHY; SEA; TEMPERATURE; THERMOMETRY; SIMULATION
AB Receptions on three vertical hydrophone arrays from basin-scale acoustic transmissions in the North Pacific during 1996 and 1998 are used to test the time-mean sound-speed properties of the World Ocean Atlas 2005 (WOA05), of an eddying unconstrained simulation of the Parallel Ocean Program (POP), and of three data-constrained solutions provided by the estimating the circulation and climate of the ocean (ECCO) project: a solution based on an approximate Kalman filter from the Jet Propulsion Laboratory (ECCO-JPL), a solution based on the adjoint method from the Massachusetts Institute of Technology (ECCO-MIT), and an eddying solution based on a Green's function approach from ECCO, Phase II (ECCO2). Predictions for arrival patterns using annual average WOA05 fields match observations to within small travel time offsets (0.3-1.0 s). Predictions for arrival patterns from the models differ substantially from the measured arrival patterns, from the WOA05 climatology, and from each other, both in terms of travel time and in the structure of the arrival patterns. The acoustic arrival patterns are sensitive to the vertical gradients of sound speed that govern acoustic propagation. Basin-scale acoustic transmissions, therefore, provide stringent tests of the vertical temperature structure of ocean state estimates. This structure ultimately influences the mixing between the surface waters and the ocean interior. The relatively good agreement of the acoustic data with the more recent ECCO solutions indicates that numerical ocean models have reached a level of accuracy where the acoustic data can provide useful additional constraints for ocean state estimation.
C1 [Dushaw, B. D.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA.
[Worcester, P. F.; Dzieciuch, M. A.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Menemenlis, D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Dushaw, BD (reprint author), Univ Washington, Appl Phys Lab, 1013 NE 40th St, Seattle, WA 98105 USA.
EM dushaw@apl.washington.edu
FU Strategic Environmental Research and Development Program through Defense
Advanced Research Projects Agency (DARPA) [MDA972-93-1-0003]; Office of
Naval Research (ONR) [N0014-1-97-1-0258, N00014-03-1-0182]; National
Oceanographic Partnership Program (NOPP); National Aeronautics and Space
Administration (NASA) Modeling Analysis and Prediction (MAP) Program;
ONR [N00014-09-1-0446, N00014-12-1-0183]
FX Our colleagues in the ATOC Consortium (A. B. Baggeroer, T. G. Birdsall,
C. Clark, J. A. Colosi, B. D. Cornuelle, D. Costa, B. D. Dushaw, M. A.
Dzieciuch, A. M. G. Forbes, C. Hill, B. M. Howe, J. Marshall, D.
Menemenlis, J. A. Mercer, K. Metzger, W. H. Munk, R. C. Spindel, D.
Stammer, P. F. Worcester, and C. Wunsch) and the NPAL Group (J. A.
Colosi, B. D. Cornuelle, B. D. Dushaw, M. A. Dzieciuch, B. M. Howe, J.
A. Mercer, W. H. Munk, R. C. Spindel, and P. F. Worcester) all
contributed in various ways to obtaining the data presented here. The
collection of the long-range acoustic data used in this work was
supported by the Strategic Environmental Research and Development
Program through Defense Advanced Research Projects Agency (DARPA) grant
MDA972-93-1-0003, by the Office of Naval Research (ONR) grants
N0014-1-97-1-0258 and N00014-03-1-0182, and by the National
Oceanographic Partnership Program (NOPP). D. Menemenlis performed this
work at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration (NASA) Modeling Analysis and Prediction (MAP) Program. B.
Dushaw was supported by ONR grants N00014-09-1-0446 and
N00014-12-1-0183.
NR 58
TC 9
Z9 9
U1 0
U2 4
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 SEP
PY 2013
VL 118
IS 9
BP 4346
EP 4362
DI 10.1002/jgrc.20325
PG 17
WC Oceanography
SC Oceanography
GA 242HQ
UT WOS:000326230200024
ER
PT J
AU Ray, RD
AF Ray, R. D.
TI Precise comparisons of bottom-pressure and altimetric ocean tides
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE tides
ID SATELLITE ALTIMETRY; GLOBAL DISTRIBUTION; BAROMETRIC TIDE; SHIDA
NUMBERS; VLBI DATA; EARTH; LOVE; ARRAY; TOPEX/POSEIDON; ATLANTIC
AB A new set of pelagic tide determinations is constructed from seafloor pressure measurements obtained at 151 sites in the deep ocean. To maximize precision of estimated tides, only stations with long time series are used; median time series length is 567 days. Geographical coverage is considerably improved by use of the international tsunami network, but coverage in the Indian Ocean and South Pacific is still weak. As a tool for assessing global ocean tide models, the data set is considerably more reliable than older data sets: the root-mean-square difference with a recent altimetric tide model is approximately 5 mm for the M-2 constituent. Precision is sufficiently high to allow secondary effects in altimetric and bottom-pressure tide differences to be studied. The atmospheric tide in bottom pressure is clearly detected at the S-1, S-2, and T-2 frequencies. The altimetric tide model is improved if satellite altimetry is corrected for crustal loading by the atmospheric tide. Models of the solid body tide can also be constrained. The free core-nutation effect in the K-1 Love number is easily detected, but the overall estimates are not as accurate as a recent determination with very long baseline interferometry.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ray, RD (reprint author), NASA, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA.
EM richard.ray@nasa.gov
RI Ray, Richard/D-1034-2012
FU National Aeronautics and Space Administration's Ocean Surface Topography
project
FX A number of scientists have contributed data to this project. I am
indebted to Doug Luther and Chris Hughes for sending tidal harmonic
constants from several recent bottom-pressure campaigns, including HOME
and RAPID. Doug Luther and Martin Guiles also reanalyzed the old BEMPEX
data. Chris Hughes, Randy Watts, and Karen Tracey provided recently
obtained BPR time series data which were included in the new tidal
analyses here. I avoided much tedious, time-consuming effort when
Andreas Macrander graciously provided his edited time series from many
of the DART stations. Jean-Paul Boy helped with analysis of atmospheric
tides. Discussions with Chris Garrett, Chris Hughes, Doug Luther, and
David Cartwright are much appreciated. This work was supported by the
National Aeronautics and Space Administration's Ocean Surface Topography
project.
NR 67
TC 28
Z9 29
U1 0
U2 14
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 SEP
PY 2013
VL 118
IS 9
BP 4570
EP 4584
DI 10.1002/jgrc.20336
PG 15
WC Oceanography
SC Oceanography
GA 242HQ
UT WOS:000326230200038
ER
PT J
AU de Steur, L
Steele, M
Hansen, E
Morison, J
Polyakov, I
Olsen, SM
Melling, H
McLaughlin, FA
Kwok, R
Smethie, WM
Schlosser, P
AF de Steur, L.
Steele, M.
Hansen, E.
Morison, J.
Polyakov, I.
Olsen, S. M.
Melling, H.
McLaughlin, F. A.
Kwok, R.
Smethie, W. M., Jr.
Schlosser, P.
TI Hydrographic changes in the Lincoln Sea in the Arctic Ocean with focus
on an upper ocean freshwater anomaly between 2007 and 2010
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE Arctic Ocean freshwater; Lincoln Sea; hydrographic observations
ID SOUTHERN CANADIAN BASIN; RIVER-RUNOFF; ICE MELTWATER; BEAUFORT GYRE;
TEMPERATURE; PACIFIC; VARIABILITY; HALOCLINE; SECTION; ORIGIN
AB Hydrographic data from the Arctic Ocean show that freshwater content in the Lincoln Sea, north of Greenland, increased significantly from 2007 to 2010, slightly lagging changes in the eastern and central Arctic. The anomaly was primarily caused by a decrease in the upper ocean salinity. In 2011 upper ocean salinities in the Lincoln Sea returned to values similar to those prior to 2007. Throughout 2008-2010, the freshest surface waters in the western Lincoln Sea show water mass properties similar to fresh Canada Basin waters north of the Canadian Arctic Archipelago. In the northeastern Lincoln Sea fresh surface waters showed a strong link with those observed in the Makarov Basin near the North Pole. The freshening in the Lincoln Sea was associated with a return of a subsurface Pacific Water temperature signal although this was not as strong as observed in the early 1990s. Comparison of repeat stations from the 2000s with the data from the 1990s at 65 degrees W showed an increase of the Atlantic temperature maximum which was associated with the arrival of warmer Atlantic water from the Eurasian Basin. Satellite-derived dynamic ocean topography of winter 2009 showed a ridge extending parallel to the Canadian Archipelago shelf as far as the Lincoln Sea, causing a strong flow toward Nares Strait and likely Fram Strait. The total volume of anomalous freshwater observed in the Lincoln Sea and exported by 2011 was close to 1100250km3, approximately 13% of the total estimated FW increase in the Arctic in 2008.
C1 [de Steur, L.] NIOZ Royal Netherlands Inst Sea Res, NL-1790 AB Den Burg, Netherlands.
[de Steur, L.; Hansen, E.] Norwegian Polar Res Inst, Tromso, Norway.
[Steele, M.; Morison, J.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA.
[Polyakov, I.] Univ Alaska Fairbanks, Int Arctic Res Ctr, Fairbanks, AK USA.
[Olsen, S. M.] Danish Meteorol Inst, Ctr Ocean & Ice, Copenhagen O, Denmark.
[Olsen, S. M.] Greenland Inst Nat Resources, Greenland Climate Res Ctr, Nuuk, Greenland.
[Melling, H.; McLaughlin, F. A.] Inst Ocean Sci, Dept Fisheries & Oceans, Sidney, BC V8L 4B2, Canada.
[Kwok, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Smethie, W. M., Jr.; Schlosser, P.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Schlosser, P.] Columbia Univ, Dept Earth & Environm Sci, New York, NY USA.
[Schlosser, P.] Columbia Univ, Dept Earth & Environm Engn, New York, NY USA.
RP de Steur, L (reprint author), NIOZ Royal Netherlands Inst Sea Res, POB 59, NL-1790 AB Den Burg, Netherlands.
EM Laura.de.Steur@nioz.nl
RI Kwok, Ron/A-9762-2008; Schlosser, Peter/C-6416-2012;
OI Kwok, Ron/0000-0003-4051-5896; Schlosser, Peter/0000-0002-6514-4203; de
Steur, Laura/0000-0002-6043-7920
FU Damocles project; European Union [GA212643, 308299]; Norwegian Research
Council; NSF [OPP02-30238, ARC06-33878, ARC10-23529, OPP-0352754,
ARC-0634226, ARC-0856330, OPP-0424864]; NASA; NOAA; Fisheries and Oceans
Canada; Canadian Program for the IPY [CC-135]
FX de Steur was funded by the Damocles project, financed by the European
Union in the 6th Framework Programme for Research and Development, the
Norwegian Research Council. Switchyard data collection and processing
was supported by NSF grants OPP02-30238, and ARC06-33878, and
ARC10-23529 to Schlosser, Smethie, and Steele. Morison was funded by NSF
OPP-0352754, NSF ARC-0634226, and NSF ARC-0856330. Polyakov was funded
by NASA, NOAA, and NSF. Olsen was funded by the European Union 7th
Framework Programme under grants agreement GA212643 and under grant
agreement 308299 NACLIM project. McLaughlin was supported by Fisheries
and Oceans Canada. The CATS study during 2007-2009 was supported by the
Canadian Program for the IPY as project CC-135. The Beaufort Gyre
program was supported by NSF OPP-0424864. The Ice-Tethered Profiler data
were collected and made available by the Ice-Tethered Profiler Program
(Toole et al., 2011; Krishfield et al., 2008) based at the Woods Hole
Oceanographic Institution (http://www.whoi.edu/itp). We thank all other
scientists, technicians, and crew involved with collecting the data that
has been used in this study.
NR 53
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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 SEP
PY 2013
VL 118
IS 9
BP 4699
EP 4715
DI 10.1002/jgrc.20341
PG 17
WC Oceanography
SC Oceanography
GA 242HQ
UT WOS:000326230200046
ER
PT J
AU Ebbets, D
Stewart, C
Spuhler, P
Atcheson, P
Van Cleve, J
Bryson, S
Clarkson, A
Barentine, J
AF Ebbets, Dennis
Stewart, Chris
Spuhler, Peter
Atcheson, Paul
Van Cleve, Jeffrey
Bryson, Stephen
Clarkson, Andrew
Barentine, John
TI Telescope with 100 square degree field-of-view for NASA's Kepler mission
SO OPTICAL ENGINEERING
LA English
DT Article
DE Kepler mission; space telescope; Schmidt telescope; photometer;
exoplanets; transits
ID TARGET STARS; 1ST; SCIENCE
AB Kepler is NASA's first space mission dedicated to the study of exoplanets. The primary scientific goal is statistical-to estimate the frequency of planetary systems associated with sun-like stars, especially the detection of earth-size planets in the habitable zones. Kepler was launched into an Earth-trailing heliocentric "drift-away"orbit (period 372 days) in March 2009. The instrument detects the faint photometric signals of transits of planets across the stellar disks of those systems with orbital planes fortuitously oriented in our line of sight. Since the probability of such alignments is small, Kepler must observe a large number of stars. In fact, Kepler is monitoring approximately 150,000 stars with a 30-min cadence. The scientific goals led to the choice of a classical Schmidt telescope, and requirements on field-of-view, throughput, spectral bandpass, image quality, scattered light, thermal and opto-mechanical stability, and in-flight adjustment authority. We review the measurement requirements, telescope design, prelaunch integration, alignment, and test program, and we describe the in-flight commissioning that optimized the performance. The stability of the flight system has enabled increasing recognition of small effects and sophistication in data processing algorithms. Astrophysical noise arising from intrinsic stellar variability is now the dominant term in the photometric error budget. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.
C1 [Ebbets, Dennis; Stewart, Chris; Spuhler, Peter; Atcheson, Paul] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA.
[Van Cleve, Jeffrey; Bryson, Stephen] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Clarkson, Andrew] L3 Integrated Opt Syst, Richmond, CA 94806 USA.
[Barentine, John] ThAcEnWIN LLC, Pittsburgh, PA 15206 USA.
RP Ebbets, D (reprint author), Ball Aerosp & Technol Corp, 1600 Commerce St, Boulder, CO 80301 USA.
EM debbets@ball.com
FU Astrophysics Division of NASA's Science Mission Directorate
FX The authors acknowledge the hundreds of scientists, engineers, and
managers from NASA Headquarters, Ames Research Center, Jet Propulsion
Laboratory, Ball Aerospace & Technologies Corp., L-3 Brashear and
Tinsley, the SETI Institute, and many universities whose dedicated
efforts over many years created the exquisite observatory that Kepler is
today. Funding was provided through the Astrophysics Division of NASA's
Science Mission Directorate.
NR 33
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PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
J9 OPT ENG
JI Opt. Eng.
PD SEP
PY 2013
VL 52
IS 9
AR 091808
DI 10.1117/1.OE.52.9.091808
PG 8
WC Optics
SC Optics
GA 241EP
UT WOS:000326149500033
ER
PT J
AU Feinberg, LD
Budinoff, J
MacEwen, H
Matthews, G
Postman, M
AF Feinberg, Lee D.
Budinoff, Jason
MacEwen, Howard
Matthews, Gary
Postman, Marc
TI Modular assembled space telescopez
SO OPTICAL ENGINEERING
LA English
DT Article
DE space telescope; James Webb Space Telescope; space assembly; deployment;
robotics; human space operations; International Space Station; libration
points
AB We present a new approach to building a modular segmented space telescope that greatly leverages the heritage of the Hubble Space Telescope and the James Webb Space Telescope. The modular design in which mirror segments are assembled into identical panels allows for economies of scale and for efficient space assembly that make a 20-m aperture approach cost effective. This assembly approach can leverage NASA's future capabilities and has the power to excite the public's imagi-nation. We discuss the science drivers, basic architecture, technology, and leveraged NASA infrastructure, concluding with a proposed plan for going forward. (C) 2013 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Feinberg, Lee D.; Budinoff, Jason] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[MacEwen, Howard] Reviresco LLC, Annandale, VA 22003 USA.
[Matthews, Gary] ITT Exelis Geospatial Syst, Greenbelt, MD 20771 USA.
[Postman, Marc] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Feinberg, LD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Lee.D.Feinberg@nasa.gov
OI Postman, Marc/0000-0002-9365-7989
NR 20
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PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
J9 OPT ENG
JI Opt. Eng.
PD SEP
PY 2013
VL 52
IS 9
AR 091802
DI 10.1117/1.OE.52.9.091802
PG 8
WC Optics
SC Optics
GA 241EP
UT WOS:000326149500027
ER
PT J
AU Fourspring, K
Ninkov, Z
Fodness, BC
Robberto, M
Heap, S
Kim, AG
AF Fourspring, Kenneth
Ninkov, Zoran
Fodness, Bryan C.
Robberto, Massimo
Heap, Sally
Kim, Alex G.
TI Proton radiation testing of digital micromirror devices for space
applications
SO OPTICAL ENGINEERING
LA English
DT Article
DE digital micromirror devices; microelectrical mechanical systems; proton
irradiation
ID MULTIOBJECT SPECTROMETER; MEMS; RELIABILITY; PERFORMANCE
AB Scientists are interested in using digital micromirror devices (DMD) as slit-masks in multiobject spectrometers on future space missions. A favored orbit is at the second Lagrangian point (L2). A requirement for mission planning is to determine how long such microelectrical mechanical systems devices would remain operational given the L2 radiation environment, which is primarily composed of solar protons and cosmic rays. To this end, we initiated DMD proton testing. Three DMDs were irradiated with high-energy protons (35 to 50 MeV) at the Lawrence Berkeley National Laboratory 88 in. Cyclotron. Assuming a typical space-craft shielding of 100 mils of aluminum, our tests imply that DMDs remain fully operable in a five-year mission at L2 with a margin of safety of 4.5. (C) 2013 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Fourspring, Kenneth; Ninkov, Zoran; Fodness, Bryan C.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Robberto, Massimo] Space Telescope Sci Inst, Baltimore, MD 21212 USA.
[Heap, Sally] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kim, Alex G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
RP Fourspring, K (reprint author), Rochester Inst Technol, 54 Lomb Mem Dr, Rochester, NY 14623 USA.
EM kdf5036@rit.edu
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PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
J9 OPT ENG
JI Opt. Eng.
PD SEP
PY 2013
VL 52
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AR 091807
DI 10.1117/1.OE.52.9.091807
PG 11
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SC Optics
GA 241EP
UT WOS:000326149500032
ER
PT J
AU Livas, JC
Arsenovic, P
Crow, JA
Hill, PC
Howard, JM
Seals, LT
Shiri, S
AF Livas, Jeffrey C.
Arsenovic, Petar
Crow, John A.
Hill, Peter C.
Howard, Joseph M.
Seals, Lenward T.
Shiri, Shahram
TI Telescopes for space-based gravitational wave missions
SO OPTICAL ENGINEERING
LA English
DT Article
DE telescopes; interferometry; laser applications; metrology; space optics;
astronomy
ID BINARIES; LISA
AB Space-based observation of gravitational waves promises to enable the study of a rich variety of high energy astrophysical sources in the 0.0001 to 1 Hz band using signals complementary to traditional electromagnetic waves. Gravitational waves represent the first new tool for studying the sky since gamma ray telescopes debuted in the 1970s, and we expect compelling science to be the result. The fundamental measurement is to monitor the path length difference between pairs of freely falling test masses with laser interferometry to a precision of picometers over gigameter baselines. The test masses are arranged in an equilateral triangle to allow simultaneous measurement of both gravitational wave polarizations. The heliocentric orbital space environment enables the test masses to be shielded from large ground motions at low frequencies, and allows the construction of long measurement baselines that are well matched to the signal wavelengths. Optical telescopes play an important role in the measurement because they deliver laser light efficiently from one spacecraft to another. The telescopes are directly in the measurement path, so there are additional performance requirements to support precision metrology beyond the usual requirements for good image formation. c 2013 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Livas, Jeffrey C.; Arsenovic, Petar; Crow, John A.; Hill, Peter C.; Howard, Joseph M.; Seals, Lenward T.; Shiri, Shahram] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Livas, JC (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Jeffrey.Livas@nasa.gov
FU NASA [11-SAT11-0027, NNH11ZDA001N]; Research Opportunities in Space and
Earth Sciences [ROSES-2011]; Strategic Astrophysics Technology (SAT)
FX The authors would like to thank P. Bender, G. Mueller, J. Sanjuan, A.
Spector, and the members of the Gravitational Wave Study Team for
support and stimulating discussions. They would also like to thank the
referees for detailed suggestions for improving the manuscript. 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).
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PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
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JI Opt. Eng.
PD SEP
PY 2013
VL 52
IS 9
AR 091811
DI 10.1117/1.OE.52.9.091811
PG 8
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SC Optics
GA 241EP
UT WOS:000326149500036
ER
PT J
AU McMurtry, C
Lee, D
Beletic, J
Chen, CYA
Demers, RT
Dorn, M
Edwall, D
Fazar, CB
Forrest, WJ
Liu, FC
Mainzer, AK
Pipher, JL
Yulius, A
AF McMurtry, Craig
Lee, Donald
Beletic, James
Chen, Chi-Yi A.
Demers, Richard T.
Dorn, Meghan
Edwall, Dennis
Fazar, Candice Bacon
Forrest, William J.
Liu, Fengchuan
Mainzer, Amanda K.
Pipher, Judith L.
Yulius, Aristo
TI Development of sensitive long-wave infrared detector arrays for
passively cooled space missions
SO OPTICAL ENGINEERING
LA English
DT Article
DE infrared; detector array; long-wave; HgCdTe; low background; passive
cooling; near earth object; dark current
ID NEAR-EARTH OBJECTS; HGCDTE; PERFORMANCE
AB The near-earth object camera (NEOCam) is a proposed infrared space mission designed to discover and characterize most of the potentially hazardous asteroids larger than 140 m in diameter that orbit near the Earth. NASA has funded technology development for NEOCam, including the development of long wavelength infrared detector arrays that will have excellent zodiacal background emission-limited performance at passively cooled focal plane temperatures. Teledyne Imaging Sensors has developed and delivered for test at the University of Rochester the first set of approximately 10 mu m cutoff, 1024 x 1024 pixel HgCdTe detector arrays. Measurements of these arrays show the development to be extremely promising: noise, dark current, quantum efficiency, and well depth goals have been met by this technology at focal plane temperatures of 35 to 40 K, readily attainable with passive cooling. The next set of arrays to be developed will address changes suggested by the first set of deliverables. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.
C1 [McMurtry, Craig; Dorn, Meghan; Fazar, Candice Bacon; Forrest, William J.; Pipher, Judith L.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Lee, Donald; Beletic, James; Chen, Chi-Yi A.; Demers, Richard T.; Edwall, Dennis; Yulius, Aristo] Teledyne Imaging Sensors, Camarillo, CA 90312 USA.
[Fazar, Candice Bacon] Roberts Wesleyan Coll, Dept Comp Sci Math & Phys, Rochester, NY 14624 USA.
[Liu, Fengchuan; Mainzer, Amanda K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP McMurtry, C (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
EM craig@pas.rochester.edu
FU NASA APRA [NNX12AF39G]
FX A. Mainzer and the JPL group acknowledge support from NASA's Discovery
program to fund development and acquisition of long-wave low-background
arrays from Teledyne, and J. Pipher and the Rochester group acknowledge
support by NASA APRA grant NNX12AF39G for test and optimization of those
arrays.
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PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
J9 OPT ENG
JI Opt. Eng.
PD SEP
PY 2013
VL 52
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AR 091804
DI 10.1117/1.OE.52.9.091804
PG 9
WC Optics
SC Optics
GA 241EP
UT WOS:000326149500029
ER
PT J
AU Oschmann, JM
Clampin, M
MacEwen, H
AF Oschmann, Jacobus M.
Clampin, Mark
MacEwen, Howard
TI Space Telescopes
SO OPTICAL ENGINEERING
LA English
DT Editorial Material
C1 [Oschmann, Jacobus M.] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA.
[Clampin, Mark] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab 667, Greenbelt, MD 20771 USA.
[MacEwen, Howard] Reviresco LLC, Annandale, VA 22003 USA.
RP Oschmann, JM (reprint author), Ball Aerosp & Technol Corp, 1600 Commerce St, Boulder, CO 80301 USA.
EM joschman@ball.com; mark.clampin@nasa.gov; howard.macewen@hmacewen.com
NR 0
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PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
J9 OPT ENG
JI Opt. Eng.
PD SEP
PY 2013
VL 52
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PG 2
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SC Optics
GA 241EP
UT WOS:000326149500026
ER
PT J
AU Stahl, HP
Henrichs, T
Luedtke, A
West, M
AF Stahl, H. Philip
Henrichs, Todd
Luedtke, Alexander
West, Miranda
TI Update to single-variable parametric cost models for space telescopes
SO OPTICAL ENGINEERING
LA English
DT Article
DE space telescope cost model; parametric cost model; cost model
AB Parametric cost models are an important tool routinely used to plan missions, compare concepts, and justify technology investments. In 2010, the article, "Single-variable parametric cost models for space telescopes," was published [H. P. Stahl et al., Opt. Eng. 49(7), 073006 (2010)]. That paper presented new single-variable cost models for space telescope optical telescope assembly. These models were created by applying standard statistical methods to data collected from 30 different space telescope missions. The results were compared with previously published models. A postpublication independent review of that paper's database identified several inconsistencies. To correct these inconsistencies, a two-year effort was undertaken to reconcile our database with source documents. This paper updates and revises the findings of our 2010 paper. As a result of the review, some telescopes' data were removed, some were revised, and data for a few new telescopes were added to the database. As a consequence, there have been changes to the 2010 published results. But our two most important findings remain unchanged: aperture diameter is the primary cost driver for large space telescopes, and it costs more per kilogram to build a low-areal-density low-stiffness telescope than a more massive high-stiffness telescope. One significant difference is that we now report telescope cost to vary linearly from 5% to 30% of total mission cost, instead of the previously reported average of 20%. To fully understand the content of this update, the authors recommend that one also read the 2010 paper. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.
C1 [Stahl, H. Philip] NASA MSFC, Huntsville, AL 35812 USA.
[Henrichs, Todd] Middle Tennessee State Univ, Dept Math Sci, Murfreesboro, TN 37132 USA.
[Luedtke, Alexander] Brown Univ, Div Appl Math, Providence, RI 02912 USA.
[West, Miranda] Univ Texas Austin, Dept Math, Austin, TX 78712 USA.
RP Stahl, HP (reprint author), NASA MSFC, Huntsville, AL 35812 USA.
EM h.philip.stahl@nasa.gov
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PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
J9 OPT ENG
JI Opt. Eng.
PD SEP
PY 2013
VL 52
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AR 091805
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PG 9
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SC Optics
GA 241EP
UT WOS:000326149500030
ER
PT J
AU Pike, A
Danner, E
Boughton, D
Melton, F
Nemani, R
Rajagopalan, B
Lindley, S
AF Pike, Andrew
Danner, Eric
Boughton, David
Melton, Forrest
Nemani, Rama
Rajagopalan, Balaji
Lindley, Steve
TI Forecasting river temperatures in real time using a stochastic dynamics
approach
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE Water Temperature; Sacramento River; uNmerical Prediction; River
Management; Heat Budget
ID STATE-SPACE MODEL; STREAM TEMPERATURE; WATER TEMPERATURES;
DISPERSION-EQUATION; NUMERICAL-SOLUTION; REGULATED RIVERS; MANAGEMENT;
CALIFORNIA; SALMON; INTERPOLATION
AB We address the growing need for accurate water temperature predictions in regulated rivers to inform decision support systems and protect aquatic habitats. Although many suitable river temperature models exist, few simultaneously model water temperature dynamics while considering uncertainty of predictions and assimilating observations. Here, we employ a stochastic dynamics approach to water temperature modeling that estimates both the water temperature state and its uncertainty by propagating error through a physically based dynamical system. This method involves converting the governing hydrodynamic and heat transport equations into a state space form and assimilating observations via the Kalman Filter. This model, called the River Assessment for Forecasting Temperature (RAFT), closes the heat budget by tracking heat movement using a robust semi-Lagrangian numerical scheme. RAFT considers key thermodynamic processes, including advection, longitudinal dispersion, atmospheric heat fluxes, lateral inflows, streambed heat exchange, and unsteady nonuniform flow. Inputs include gridded meteorological forecasts from a numerical weather prediction model, bathymetric cross-sectional geometry, and temperature and flow measurements at the upstream boundary and tributaries. We applied RAFT to an approximate to 100 km portion of the Sacramento River in California, downstream of Keswick Dam (a regulatory dam below Shasta Dam), at a spatial resolution of 2 km and a temporal resolution of 15 min. Model prediction error over a 6 month calibration period was on the order of 0.5 degrees C. When temperature and flow gage data were assimilated, the mean prediction error was significantly less (0.25 degrees C). The model accurately predicts the magnitude and timing of diel temperature fluctuations and can provide 72 h water temperature forecasts when linked with meteorological forecasts and real-time flow/temperature monitoring networks. RAFT is potentially scalable to model and forecast fine-grained one-dimensional temperature dynamics covering a broad extent in a variety of regulated rivers provided that adequate input data are available.
C1 [Pike, Andrew] Univ Calif Santa Cruz, Inst Marine Sci, Santa Cruz, CA 95064 USA.
[Pike, Andrew; Danner, Eric; Boughton, David; Lindley, Steve] NOAA, Fisheries Ecol Div, Natl Marine Fisheries Serv, Santa Cruz, CA 95060 USA.
[Melton, Forrest; Nemani, Rama] NASA, Ames Res Ctr, Biospher Sci Branch, Moffett Field, CA 94035 USA.
[Melton, Forrest] Calif State Univ Monterey Bay, Dept Sci & Environm Policy, Seaside, CA USA.
[Rajagopalan, Balaji] Univ Colorado, Dept Environm & Architectural Engn, Boulder, CO 80309 USA.
RP Pike, A (reprint author), NOAA, Fisheries Ecol Div, Natl Marine Fisheries Serv, 110 Shaffer Rd, Santa Cruz, CA 95060 USA.
EM andrew.pike@noaa.gov
RI Lindley, Steven/G-3997-2014; Rajagopalan, Balaji/A-5383-2013
OI Lindley, Steven/0000-0001-9556-0411; Rajagopalan,
Balaji/0000-0002-6883-7240
FU NASA Applied Sciences award [NNX08AK72G]; NOAA/NMFS Southwest Fisheries
Science Center
FX Funding for this study was provided by NASA Applied Sciences award
NNX08AK72G and by the NOAA/NMFS Southwest Fisheries Science Center.
NR 61
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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 SEP
PY 2013
VL 49
IS 9
BP 5168
EP 5182
DI 10.1002/wrcr.20389
PG 15
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 238ZO
UT WOS:000325991100005
ER
PT J
AU Baugh, CA
Bates, PD
Schumann, G
Trigg, MA
AF Baugh, Calum A.
Bates, Paul D.
Schumann, Guy
Trigg, Mark A.
TI SRTM vegetation removal and hydrodynamic modeling accuracy
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE SRTM DEM accuracy; global vegetation height data set; remote sensing;
hydrodynamic modeling; Amazon River
ID RADAR TOPOGRAPHY MISSION; AMAZON BASIN; HYDRAULIC MODELS; C-BAND;
INUNDATION; VALIDATION; ALTIMETRY; RELIEF; DEM; GEOMORPHOLOGY
AB Hydrodynamic modeling of large remote forested floodplains, such as the Amazon, is hindered by the vegetation signal contained within Digital Elevation Models (DEMs) such as the Shuttle Radar Topography Mission (SRTM). Not removing the vegetation signal causes DEMs to be overelevated preventing the correct simulation of overbank inundation. Previous efforts to remove this vegetation signal have either not accounted for its spatial variability or relied upon single assumed error values. As a possible solution, a systematic approach to removing the vegetation signal which accounts for spatial variability using recently published estimates of global vegetation heights is proposed. The proposed approach is applied to a well-studied reach of the Amazon floodplain where previous hydrodynamic model applications were affected by the SRTM vegetation signal. Greatest improvements to hydrodynamic model accuracy were obtained by subtracting 50-60% of the vegetation height from the SRTM. The vegetation signal removal procedure improved the RMSE (Root-Mean-Square Error) accuracy of the hydrodynamic model than when using the original SRTM in three ways: (1) seasonal floodplain water elevation predictions against TOPEX/Poseidon observations improved from 6.61 to 1.84 m; (2) high water inundation extent prediction accuracy improved from 0.52 to 0.07 against a JERS (Japanese Earth Resources Satellite) observation; (3) low water inundation extent accuracy against a JERS observation improved from 0.22 to 0.12. The simple data requirements of this vegetation removal method enable it to be applied to any remote floodplain for which hydrodynamic model accuracy is hindered by vegetation present in the DEM.
C1 [Baugh, Calum A.; Bates, Paul D.; Trigg, Mark A.] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
[Schumann, Guy] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Baugh, CA (reprint author), Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
EM calum.baugh@bristol.ac.uk
RI Schumann, Guy/F-9760-2011; Bates, Paul/C-8026-2012; Trigg,
Mark/A-5898-2010
OI Bates, Paul/0000-0001-9192-9963; Trigg, Mark/0000-0002-8412-9332
FU U.K. Natural Environment Research Council; Willis Research Network;
National Aeronautics and Space Administration
FX We would like to acknowledge ANA Hidro-web for providing Amazon gauge
data. All simulations in this study were performed using the
computational facilities of the Advanced Computing Research Centre,
University of Bristol-http://www.bris.ac.uk/acrc/. Calum Baugh is
supported by a studentship funded by the U.K. Natural Environment
Research Council. Mark Trigg is a Willis Research Fellow and the
contribution to this paper was completed under funding provided by the
Willis Research Network. Guy Schumann's time at the Jet Propulsion
Laboratory, California Institute of Technology, was funded under a
contract with the National Aeronautics and Space Administration. We
thank the three anonymous reviewers who provided very useful comments
which have significantly improved the manuscript.
NR 53
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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 SEP
PY 2013
VL 49
IS 9
BP 5276
EP 5289
DI 10.1002/wrcr.20412
PG 14
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 238ZO
UT WOS:000325991100012
ER
PT J
AU Allwood, AC
Burch, IW
Rouchy, JM
Coleman, M
AF Allwood, A. C.
Burch, I. W.
Rouchy, J. M.
Coleman, M.
TI Morphological Biosignatures in Gypsum: Diverse Formation Processes of
Messinian (similar to 6.0 Ma) Gypsum Stromatolites
SO ASTROBIOLOGY
LA English
DT Article
DE Stromatolites; Gypsum; Evaporites; Mars; Biosignature
ID MERIDIANI-PLANUM; SALINITY CRISIS; BURNS FORMATION; EVAPORITE;
PRECIPITATION; BASIN; MICROFOSSILS; ASSEMBLAGES; SELENITE; CALCITE
AB The approximate to 5.3-6.0 million-year-old evaporitic gypsum deposits of Cyprus and Crete contain a variety of stromatolites that formed during the Messinian salinity crisis. We recognize four stromatolite morphotypes, including domical, conical, columnar, and flat-laminated structures. Observations of morphological and textural variations among the different morphotypes reveal significant diversity and complexity in the nature of interactions between microorganisms, gypsum deposition, and gypsum crystal growth. Nonbiological processes (detrital gypsum deposition, in situ crust precipitation, syntaxial crystal growth, subsurface crystal growth, and recrystallization) interacted with inferred microbial processes (including localized growth of biofilms, trapping and binding of grains in mats, nucleation of gypsum on cells) to produce distinct morphological-textural assemblages. Evidence for biological origins is clear in some stromatolite morphotypes and can come from the presence of microfossils, the spatial distribution of organic matter, and stromatolite morphology. In one stromatolite morphotype, the presence of the stromatolite, or the biota associated with it, may have determined the morphology of gypsum crystals. In some stromatolite morphotypes, definitive evidence of a microbial influence is not as clear. There are broad similarities between the Messinian gypsum stromatolites and carbonate stromatolites elsewhere in the geologic record, such as the formation of precipitated and granular layers; the development of domed, columnar, and conical morphotypes; the potential for microbes to influence mineral precipitation; and the recrystallization of deposits during burial. However, in detail the array of microbial-sedimentary-diagenetic process interactions is quite distinct in gypsiferous systems due to differences in the way gypsum typically forms and evolves in the paleoenvironment compared to carbonate. Unique aspects of the taphonomy of gypsum compared to carbonate chemical sediments, generally speaking, include the following: the potential for growth of individual crystals to determine the shape of a stromatolite (and possibly vice versa), a more diverse set of outcomes relating to preservation versus destruction of textures through crystal growth and recrystallization, and a greater likelihood of preserving microfossils through encapsulation in large crystals. These insights gained from the study of terrestrial gypsum sedimentary rocks provide valuable guidance for the search for clues to past life in sulfate chemical sediments on Mars.
C1 [Allwood, A. C.; Coleman, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Burch, I. W.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW, Australia.
[Rouchy, J. M.] Museum Natl Hist Nat, Dept Hist Terre, F-75231 Paris, France.
[Coleman, M.] NASA Astrobiol Inst WARC, Pasadena, CA USA.
RP Allwood, AC (reprint author), CALTECH, Jet Prop Lab, MS183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM abigail.c.allwood@jpl.nasa.gov
FU National Aeronautics and Space Administration; Research and Technology
Development Program; NASA Postdoctoral Program; NASA Astrobiology
Institute (NAI-WARC)
FX 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 and funded through the Research and
Technology Development Program, the NASA Postdoctoral Program, and the
NASA Astrobiology Institute (NAI-WARC). (C) 2013 All rights reserved.
The authors are grateful to the Geological Survey of Greece and the
Geological Survey of Cyprus for helpful discussions and provision of
access to the field sites.
NR 63
TC 10
Z9 10
U1 4
U2 23
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
EI 1557-8070
J9 ASTROBIOLOGY
JI Astrobiology
PD SEP 1
PY 2013
VL 13
IS 9
BP 870
EP 886
DI 10.1089/ast.2013.1021
PG 17
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 219TU
UT WOS:000324534100007
PM 24047112
ER
PT J
AU Goswami, I
Peelukhana, SV
Al-Rjoub, MF
Back, LH
Banerjee, RK
AF Goswami, Ishan
Peelukhana, Srikara V.
Al-Rjoub, Marwan F.
Back, Lloyd H.
Banerjee, Rupak K.
TI Influence of Variable Native Arterial Diameter and Vasculature Status on
Coronary Diagnostic Parameters
SO JOURNAL OF BIOMECHANICAL ENGINEERING-TRANSACTIONS OF THE ASME
LA English
DT Article
DE stenosis; coronary diagnostic parameters; native diameter; myocardial
infarction; fractional flow reserve; pressure drop coefficient
ID FRACTIONAL FLOW RESERVE; RATE-PRESSURE-DROP; BLOOD-FLOW;
MYOCARDIAL-INFARCTION; MICROVASCULAR DYSFUNCTION; IN-VITRO;
PHYSIOLOGICAL ASSESSMENT; STENOSIS SEVERITY; ANGIOPLASTY; HUMANS
AB In current practice, diagnostic parameters, such as fractional flow reserve (FFR) and coronary flow reserve (CFR), are used to determine the severity of a coronary artery stenosis. FFR is defined as the ratio of hyperemic pressures distal ((p) over bar (rh)) and proximal ((p) over bar (ah)) to a stenosis. CFR is the ratio of flow at hyperemic and basal condition. Another diagnostic parameter suggested by our group is the pressure drop coefficient (CDP). CDP is defined as the ratio of the pressure drop across the stenosis to the upstream dynamic pressure. These parameters are evaluated by invasively measuring flow (CFR), pressure (FFR), or both (CDP) in a diseased artery using guidewire tipped with a sensor. Pathologic state of artery is indicated by lower CFR (<2). Similarly, FFR lower than 0.75 leads to clinical intervention. Cutoff for CDP is under investigation. Diameter and vascular condition influence both flow and pressure drop, and thus, their effect on FFR and CDP was studied. In vitro experiment coupled with pressure-flow relationships from human clinical data was used to simulate pathophysiologic conditions in two representative arterial diameters, 2.5mm (N1) and 3mm (N2). With a 0.014 in. (0.35 mm) guidewire inserted, diagnostic parameters were evaluated for mild (similar to 64% area stenosis (AS)), intermediate (similar to 80% AS), and severe (similar to 90% AS) stenosis for both N1 and N2 arteries, and between two conditions, with and without myocardial infarction (MI). Arterial diameter did not influence FFR for clinically relevant cases of mild and intermediate stenosis (difference <5%). Stenosis severity was underestimated due to higher FFR (mild: similar to 9%, intermediate: similar to 20%, severe: similar to 30%) for MI condition because of lower pressure drops, and this may affect clinical decision making. CDP varied with diameter (mild: similar to 20%, intermediate: similar to 24%, severe: by 2.5 times), and vascular condition (mild: similar to 35%, intermediate: similar to 14%, severe: similar to 9%). However, nonoverlapping range of CDP allowed better delineation of stenosis severities irrespective of diameter and vascular condition.
C1 [Goswami, Ishan; Peelukhana, Srikara V.; Al-Rjoub, Marwan F.; Banerjee, Rupak K.] Univ Cincinnati, Sch Dynam Syst, Mech Engn Program, Cincinnati, OH 45221 USA.
[Back, Lloyd H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Banerjee, RK (reprint author), Univ Cincinnati, Sch Dynam Syst, Mech Engn Program, Cincinnati, OH 45221 USA.
EM Rupak.banerjee@uc.edu
FU ACIST Medical System [G400924-6200600000-1-1008190]
FX The study was partially funded by ACIST Medical System (Grant No.
G400924-6200600000-1-1008190). The authors would also like to
acknowledge the help from Tri-State Tool Grinding, Cincinnati, Ohio.
NR 51
TC 3
Z9 3
U1 1
U2 4
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0148-0731
EI 1528-8951
J9 J BIOMECH ENG-T ASME
JI J. Biomech. Eng.-Trans. ASME
PD SEP
PY 2013
VL 135
IS 9
AR 091005
DI 10.1115/1.4024682
PG 8
WC Biophysics; Engineering, Biomedical
SC Biophysics; Engineering
GA 240HJ
UT WOS:000326085700005
PM 23817842
ER
PT J
AU Szabados, L
Anderson, RI
Derekas, A
Kiss, LL
Szalai, T
Szekely, P
Christiansen, JL
AF Szabados, L.
Anderson, R. I.
Derekas, A.
Kiss, L. L.
Szalai, T.
Szekely, P.
Christiansen, J. L.
TI Discovery of the spectroscopic binary nature of three bright southern
Cepheids
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: spectroscopic; stars: variables: Cepheids
ID GALACTIC CEPHEIDS; PERIOD CEPHEIDS; VARIABLE-STARS; PHOTOMETRY;
COMPANIONS; HEMISPHERE
AB We present an analysis of spectroscopic radial velocity and photometric data of three bright Galactic Cepheids: LR Trianguli Australis (LR TrA), RZ Velorum (RZ Vel) and BG Velorum (BG Vel). Based on new radial velocity data, these Cepheids have been found to be members of spectroscopic binary systems. The ratio of the peak-to-peak radial velocity amplitude to photometric amplitude indicates the presence of a companion for LR TrA and BG Vel. IUE spectra indicate that the companions of RZ Vel and BG Vel cannot be hot stars. The analysis of all available photometric data revealed that the pulsation period of RZ Vel and BG Vel varies monotonically, due to stellar evolution. Moreover, the longest period Cepheid in this sample, RZ Vel, shows period fluctuations superimposed on the monotonic period increase. The light-time effect interpretation of the observed pattern needs long-term photometric monitoring of this Cepheid. The pulsation period of LR TrA has remained constant since the discovery of its brightness variation. Using statistical data, it is also shown that a large number of spectroscopic binaries still remain to be discovered among bright classical Cepheids.
C1 [Szabados, L.; Derekas, A.; Kiss, L. L.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1121 Budapest, Hungary.
[Anderson, R. I.] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland.
[Derekas, A.; Kiss, L. L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Kiss, L. L.] ELTE Gothard Lendulet Res Grp, H-9700 Szombathely, Hungary.
[Szalai, T.] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary.
[Szekely, P.] Univ Szeged, Dept Expt Phys, H-6720 Szeged, Hungary.
[Christiansen, J. L.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Szabados, L (reprint author), Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary.
EM szabados@konkoly.hu
RI Derekas, Aliz/G-2091-2016;
OI Derekas, Aliz/0000-0002-6526-9444; Anderson, Richard
I./0000-0001-8089-4419
FU ESTEC [4000106398/12/NL/KML]; Hungarian OTKA [K76816, K83790, K104607,
MB08C 81013]; European Community [269194]; Hungarian Academy of
Sciences; Hungarian Eotvos Fellowship; Janos Bolyai Research Scholarship
of the Hungarian Academy of Sciences; European Research Council under
the European Community [227224]
FX This project has been supported by ESTEC Contract No.
4000106398/12/NL/KML, Hungarian OTKA Grants K76816, K83790, K104607 and
MB08C 81013, as well as the European Community's Seventh Framework
Program (FP7/2007-2013) under grant agreement no. 269194, and the
'Lendulet-2009' Young Researchers Program of the Hungarian Academy of
Sciences. AD was supported by a Hungarian Eotvos Fellowship. AD has also
been supported by a Janos Bolyai Research Scholarship of the Hungarian
Academy of Sciences. AD is very thankful to the staff at The Lodge in
the Siding Spring Observatory for their hospitality and very nice food,
making the time spent there lovely and special. Part of the research
leading to these results has received funding from the European Research
Council under the European Community's Seventh Framework Program
(FP7/2007-2013)/ERC grant agreement no. 227224 (PROSPERITY). The
INTEGRAL photometric data, pre-processed by ISDC, have been retrieved
from the OMC Archive at CAB (INTA-CSIC). We are indebted to Stanley
Walker for sending us some unpublished photoelectric observational data.
Our thanks are also due to the referee and Dr Maria Kun for their
critical remarks leading to a considerable improvement in the
presentation of the results.
NR 40
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 SEP
PY 2013
VL 434
IS 1
BP 870
EP 877
DI 10.1093/mnras/stt1079
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 207XA
UT WOS:000323636800063
ER
PT J
AU Ade, PAR
Aghanim, N
Alves, MIR
Arnaud, M
Ashdown, M
Atrio-Barandela, F
Aumont, J
Baccigalupi, C
Balbi, A
Banday, AJ
Barreiro, RB
Bartlett, JG
Battaner, E
Bedini, L
Benabed, K
Benoit, A
Bernard, JP
Bersanelli, M
Bonaldi, A
Bond, JR
Borrill, J
Bouchet, FR
Boulanger, F
Burigana, C
Butler, RC
Cabella, P
Cardoso, JF
Chen, X
Chiang, LY
Christensen, PR
Clements, DL
Colombi, S
Colombo, LPL
Coulais, A
Cuttaia, F
Davies, RD
Davis, RJ
de Bernardis, P
de Gasperis, G
de Zotti, G
Delabrouille, J
Dickinson, C
Diego, JM
Dobler, G
Dole, H
Donzelli, S
Dore, O
Douspis, M
Dupac, X
Ensslin, TA
Finelli, F
Forni, O
Frailis, M
Franceschi, E
Galeotta, S
Ganga, K
Genova-Santos, RT
Ghosh, T
Giard, M
Giardino, G
Giraud-Heraud, Y
Gonzalez-Nuevo, J
Gorski, KM
Gregorio, A
Gruppuso, A
Hansen, FK
Harrison, D
Hernandez-Monteagudo, C
Hildebrandt, SR
Hivon, E
Hobson, M
Holmes, WA
Hornstrup, A
Hovest, W
Huffenberger, KM
Jaffe, TR
Jaffe, AH
Juvela, M
Keihanen, E
Keskitalo, R
Kisner, TS
Knoche, J
Kunz, M
Kurki-Suonio, H
Lagache, G
Lahteenmaki, A
Lamarre, JM
Lasenby, A
Lawrence, CR
Leach, S
Leonardi, R
Lilje, PB
Linden-Vornle, M
Lubin, PM
Macias-Perez, JF
Maffei, B
Maino, D
Mandolesi, N
Maris, M
Marshall, DJ
Martin, PG
Martinez-Gonzalez, E
Masi, S
Massardi, M
Matarrese, S
Mazzotta, P
Melchiorri, A
Mennella, A
Mitra, S
Miville-Deschenes, MA
Moneti, A
Montier, L
Morgante, G
Mortlock, D
Munshi, D
Murphy, JA
Naselsky, P
Nati, F
Natoli, P
Norgaard-Nielsen, HU
Noviello, F
Novikov, D
Novikov, I
Osborne, S
Oxborrow, CA
Pajot, F
Paladini, R
Paoletti, D
Peel, M
Perotto, L
Perrotta, F
Piacentini, F
Piat, M
Pierpaoli, E
Pietrobon, D
Plaszczynski, S
Pointecouteau, E
Polenta, G
Popa, L
Poutanen, T
Pratt, GW
Prunet, S
Puget, JL
Rachen, JP
Reach, WT
Rebolo, R
Reinecke, M
Renault, C
Ricciardi, S
Ristorcelli, I
Rocha, G
Rosset, C
Rubino-Martin, JA
Rusholme, B
Salerno, E
Sandri, M
Savini, G
Scott, D
Spencer, L
Stolyarov, V
Sudiwala, R
Suur-Uski, AS
Sygnet, JF
Tauber, JA
Terenzi, L
Tibbs, CT
Toffolatti, L
Tomasi, M
Tristram, M
Valenziano, L
Van Tent, B
Varis, J
Vielva, P
Villa, F
Vittorio, N
Wade, LA
Wandelt, BD
Ysard, N
Yvon, D
Zacchei, A
Zonca, A
AF Ade, P. A. R.
Aghanim, N.
Alves, M. I. R.
Arnaud, M.
Ashdown, M.
Atrio-Barandela, F.
Aumont, J.
Baccigalupi, C.
Balbi, A.
Banday, A. J.
Barreiro, R. B.
Bartlett, J. G.
Battaner, E.
Bedini, L.
Benabed, K.
Benoit, A.
Bernard, J. -P.
Bersanelli, M.
Bonaldi, A.
Bond, J. R.
Borrill, J.
Bouchet, F. R.
Boulanger, F.
Burigana, C.
Butler, R. C.
Cabella, P.
Cardoso, J. -F.
Chen, X.
Chiang, L. -Y
Christensen, P. R.
Clements, D. L.
Colombi, S.
Colombo, L. P. L.
Coulais, A.
Cuttaia, F.
Davies, R. D.
Davis, R. J.
de Bernardis, P.
de Gasperis, G.
de Zotti, G.
Delabrouille, J.
Dickinson, C.
Diego, J. M.
Dobler, G.
Dole, H.
Donzelli, S.
Dore, O.
Douspis, M.
Dupac, X.
Ensslin, T. A.
Finelli, F.
Forni, O.
Frailis, M.
Franceschi, E.
Galeotta, S.
Ganga, K.
Genova-Santos, R. T.
Ghosh, T.
Giard, M.
Giardino, G.
Giraud-Heraud, Y.
Gonzalez-Nuevo, J.
Gorski, K. M.
Gregorio, A.
Gruppuso, A.
Hansen, F. K.
Harrison, D.
Hernandez-Monteagudo, C.
Hildebrandt, S. R.
Hivon, E.
Hobson, M.
Holmes, W. A.
Hornstrup, A.
Hovest, W.
Huffenberger, K. M.
Jaffe, T. R.
Jaffe, A. H.
Juvela, M.
Keihanen, E.
Keskitalo, R.
Kisner, T. S.
Knoche, J.
Kunz, M.
Kurki-Suonio, H.
Lagache, G.
Lahteenmaki, A.
Lamarre, J. -M.
Lasenby, A.
Lawrence, C. R.
Leach, S.
Leonardi, R.
Lilje, P. B.
Linden-Vornle, M.
Lubin, P. M.
Macias-Perez, J. F.
Maffei, B.
Maino, D.
Mandolesi, N.
Maris, M.
Marshall, D. J.
Martin, P. G.
Martinez-Gonzalez, E.
Masi, S.
Massardi, M.
Matarrese, S.
Mazzotta, P.
Melchiorri, A.
Mennella, A.
Mitra, S.
Miville-Deschenes, M. -A.
Moneti, A.
Montier, L.
Morgante, G.
Mortlock, D.
Munshi, D.
Murphy, J. A.
Naselsky, P.
Nati, F.
Natoli, P.
Norgaard-Nielsen, H. U.
Noviello, F.
Novikov, D.
Novikov, I.
Osborne, S.
Oxborrow, C. A.
Pajot, F.
Paladini, R.
Paoletti, D.
Peel, M.
Perotto, L.
Perrotta, F.
Piacentini, F.
Piat, M.
Pierpaoli, E.
Pietrobon, D.
Plaszczynski, S.
Pointecouteau, E.
Polenta, G.
Popa, L.
Poutanen, T.
Pratt, G. W.
Prunet, S.
Puget, J. -L.
Rachen, J. P.
Reach, W. T.
Rebolo, R.
Reinecke, M.
Renault, C.
Ricciardi, S.
Ristorcelli, I.
Rocha, G.
Rosset, C.
Rubino-Martin, J. A.
Rusholme, B.
Salerno, E.
Sandri, M.
Savini, G.
Scott, D.
Spencer, L.
Stolyarov, V.
Sudiwala, R.
Suur-Uski, A. -S.
Sygnet, J. -F.
Tauber, J. A.
Terenzi, L.
Tibbs, C. T.
Toffolatti, L.
Tomasi, M.
Tristram, M.
Valenziano, L.
Van Tent, B.
Varis, J.
Vielva, P.
Villa, F.
Vittorio, N.
Wade, L. A.
Wandelt, B. D.
Ysard, N.
Yvon, D.
Zacchei, A.
Zonca, A.
TI Planck intermediate results. XII: Diffuse Galactic components in the
Gould Belt system
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Galaxy: general; radio continuum: ISM; radiation mechanisms: general
ID MICROWAVE-ANISOTROPY-PROBE; SPINNING DUST EMISSION; CENTIMETER-WAVE
CONTINUUM; H-ALPHA; INFRARED-EMISSION; WMAP OBSERVATIONS; ANOMALOUS
DUST; FOREGROUND EMISSION; TENTATIVE DETECTION; POLARIZATION DATA
AB We perform an analysis of the diffuse low-frequency Galactic components in the southern part of the Gould Belt system (130 degrees <= l <= 230 degrees and -50 degrees <= b <= -10 degrees). Strong ultra-violet flux coming from the Gould Belt super-association is responsible for bright diffuse foregrounds that we observe from our position inside the system and that can help us improve our knowledge of the Galactic emission. Free-free emission and anomalous microwave emission (AME) are the dominant components at low frequencies (nu < 40 GHz), while synchrotron emission is very smooth and faint. We separated diffuse free-free emission and AME from synchrotron emission and thermal dust emission by using Planck data, complemented by ancillary data, using the correlated component analysis (CCA) component-separation method and we compared our results with the results of cross-correlation of foreground templates with the frequency maps. We estimated the electron temperature T-e from Ha and free-free emission using two methods (temperature-temperature plot and cross-correlation) and obtained T-e ranging from 3100 to 5200 K for an effective fraction of absorbing dust along the line of sight of 30% (f(d) = 0.3). We estimated the frequency spectrum of the diffuse AME and recovered a peak frequency (in flux density units) of 25.5 +/- 1.5 GHz. We verified the reliability of this result with realistic simulations that include biases in the spectral model for the AME and in the free-free template. By combining physical models for vibrational and rotational dust emission and adding the constraints from the thermal dust spectrum from Planck and IRAS, we are able to present a good description of the AME frequency spectrum for plausible values of the local density and radiation field.
C1 [Bartlett, J. G.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Piat, M.; Rosset, C.] Univ Paris Diderot, APC, CNRS, IN2P3,CEA,Irfu,Observ Paris, F-75205 Paris 13, France.
[Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland.
[Kunz, M.] African Inst Math Sci, Cape Town, South Africa.
[Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy.
[Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy.
[Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 OHE, England.
[Bond, J. R.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Bedini, L.; Salerno, E.] CNR, ISTI, Area Ric, Pisa, Italy.
[Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Dore, O.; Hildebrandt, S. R.; Rocha, G.] CALTECH, Pasadena, CA 91125 USA.
[Hernandez-Monteagudo, C.] CEFCA, Teruel 44001, Spain.
[Borrill, J.; Keskitalo, R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Comp Cosmol Ctr, Berkeley, CA 94720 USA.
[Rebolo, R.] CSIC, Madrid, Spain.
[Yvon, D.] CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France.
[Hornstrup, A.; Linden-Vornle, M.; Norgaard-Nielsen, H. U.; Oxborrow, C. A.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Kgs, Denmark.
[Kunz, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland.
[Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain.
[Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain.
[Rachen, J. P.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
[Keskitalo, R.] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA.
[Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.; Ysard, N.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Matarrese, S.] Univ Padua, Dipartimento Fis Astron G Galilei, I-35131 Padua, Italy.
[Burigana, C.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis Sci Terra, I-44122 Ferrara, Italy.
[de Bernardis, P.; Masi, S.; Melchiorri, A.; Nati, F.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Bersanelli, M.; Maino, D.; Mennella, A.] Univ Milan, Dipartimento Fis, Milan, Italy.
[Gregorio, A.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Balbi, A.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy.
[Cabella, P.] Univ Roma Tor Vergata, Dipartimento Matemat, I-00133 Rome, Italy.
[Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark.
[Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, Tenerife 38206, Spain.
[Dupac, X.; Leonardi, R.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain.
[Giardino, G.; Tauber, J. A.] European Space Agcy, ESTEC, NL-2201 AZ Noordwijk, Netherlands.
[Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.; Suur-Uski, A. -S.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland.
[de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy.
[Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Frailis, M.; Galeotta, S.; Gregorio, A.; Maris, M.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Massardi, M.] Ist Radioastron, INAF, I-40129 Bologna, Italy.
[Burigana, C.; Butler, R. C.; Cuttaia, F.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] IASF Bologna, INAF, Bologna, Italy.
[Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Tomasi, M.] IASF Milano, INAF, Milan, Italy.
[Finelli, F.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy.
[Melchiorri, A.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy.
[Mitra, S.] IUCAA, Pune 411007, Maharashtra, India.
[Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Imperial Coll London, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Chen, X.; Paladini, R.; Rusholme, B.; Tibbs, C. T.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France.
[Dole, H.] Inst Univ France, F-75005 Paris, France.
[Aghanim, N.; Alves, M. I. R.; Aumont, J.; Boulanger, F.; Dole, H.; Douspis, M.; Ghosh, T.; Kunz, M.; Lagache, G.; Miville-Deschenes, M. -A.; Pajot, F.; Puget, J. -L.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France.
[Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Popa, L.] Inst Space Sci, Bucharest, Romania.
[Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Harrison, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway.
[Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain.
[Barreiro, R. B.; Diego, J. M.; Gonzalez-Nuevo, J.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain.
[Bartlett, J. G.; Colombo, L. P. L.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Pietrobon, D.; Rocha, G.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bonaldi, A.; Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.; Noviello, F.; Peel, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Ashdown, M.; Harrison, D.; Lasenby, A.; Stolyarov, V.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
[Dobler, G.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS, IN2P3, LAL, F-91405 Orsay, France.
[Coulais, A.; Lamarre, J. -M.] CNRS, LERMA, Observ Paris, Paris, France.
[Arnaud, M.; Marshall, D. J.; Pratt, G. W.] Univ Paris Diderot, CNRS, CEA Saclay, CEA DSM,Lab AIM,IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France.
[Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France.
[Macias-Perez, J. F.; Perotto, L.; Renault, C.] Univ Grenoble 1, CNRS, IN2P3, Inst Natl Polytech Grenoble,Lab Phys Subat & Cosm, F-38026 Grenoble, France.
[Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France.
[Van Tent, B.] CNRS, F-91405 Orsay, France.
[Kisner, T. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Rachen, J. P.; Reinecke, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland.
[Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland.
[Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Savini, G.] UCL, Opt Sci Lab, London, England.
[Baccigalupi, C.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Ade, P. A. R.; Munshi, D.; Spencer, L.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Zelenchukskiy Region 369167, Karachai Cherke, Russia.
[Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Benabed, K.; Bouchet, F. R.; Colombi, S.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UPMC, UMR 7095, F-75014 Paris, France.
[Banday, A. J.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA.
[Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain.
[Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Bonaldi, A (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England.
EM anna.bonaldi@manchester.ac.uk
RI Butler, Reginald/N-4647-2015; Ghosh, Tuhin/E-6899-2016; Tomasi,
Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo,
Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012;
Piacentini, Francesco/E-7234-2010; Atrio-Barandela,
Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Mazzotta,
Pasquale/B-1225-2016; Salerno, Emanuele/A-2137-2010; Bouchet,
Francois/B-5202-2014; Lahteenmaki, Anne/L-5987-2013; Vielva,
Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Battaner,
Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon,
Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015;
Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015;
Novikov, Dmitry/P-1807-2015; Kurki-Suonio, Hannu/B-8502-2016
OI Paoletti, Daniela/0000-0003-4761-6147; Savini,
Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993;
TERENZI, LUCA/0000-0001-9915-6379; Reach, William/0000-0001-8362-4094;
Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192;
Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794;
Burigana, Carlo/0000-0002-3005-5796; Bouchet,
Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043;
Villa, Fabrizio/0000-0003-1798-861X; Peel, Mike/0000-0003-3412-2586;
Galeotta, Samuele/0000-0002-3748-5115; Finelli,
Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis,
Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta,
Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996;
Sandri, Maura/0000-0003-4806-5375; Cuttaia,
Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099;
Masi, Silvia/0000-0001-5105-1439; de Bernardis,
Paolo/0000-0001-6547-6446; Forni, Olivier/0000-0001-6772-9689; Morgante,
Gianluca/0000-0001-9234-7412; Maris, Michele/0000-0001-9442-2754;
Franceschi, Enrico/0000-0002-0585-6591; Valenziano,
Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Tomasi,
Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati,
Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327;
Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov,
Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748;
WANDELT, Benjamin/0000-0002-5854-8269; Rubino-Martin, Jose
Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595;
Salerno, Emanuele/0000-0002-3433-3634; Vielva,
Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386;
Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez,
Enrique/0000-0002-0179-8590; Gonzalez-Nuevo,
Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292;
Kurki-Suonio, Hannu/0000-0002-4618-3063
FU ESA Member States; NASA; ESA; CNES; CNRS/INSU-IN2P3-INP (France); ASI;
CNR; INAF (Italy); DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA; RES
(Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada);
DTU Space (Denmark); SER/SSO (Switzerland);; RCN (Norway); SFI
(Ireland); FCT/MCTES (Portugal)
FX Based on observations obtained with Planck (http://www.esa.int/Planck),
an ESA science mission with instruments and contributions directly
funded by ESA Member States, NASA, and Canada. The development of Planck
has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI,
CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC,
MICINN, 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); and the development of
Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP
(France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA
(UK); CSIC, MICINN and JA (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); and PRACE (EU). A
description of the Planck Collaboration and a list of its members,
including the technical or scientific activities in which they have been
involved, can be found at
http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabora
tion. We acknowledge the use of the HEALPix (Gorski et al. 2005) package
and of the LAMBDA website http://lambda.gsfc.nasa.gov.
NR 94
TC 8
Z9 8
U1 2
U2 25
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 SEP
PY 2013
VL 557
AR A53
DI 10.1051/0004-6361/201321160
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 228TC
UT WOS:000325211900040
ER
PT J
AU Ade, PAR
Aghanim, N
Arnaud, M
Ashdown, M
Atrio-Barandela, F
Aumont, J
Baccigalupi, C
Balbi, A
Banday, AJ
Barreiro, RB
Barrena, R
Bartlett, JG
Battaner, E
Benabed, K
Bernard, JP
Bersanelli, M
Bikmaev, I
Bock, JJ
Bohringer, H
Bonaldi, A
Bond, JR
Borrill, J
Bouchet, FR
Bourdin, H
Burenin, R
Burigana, C
Butler, RC
Cabella, P
Chamballu, A
Chary, RR
Chiang, LY
Chon, G
Christensen, PR
Clements, DL
Colafrancesco, S
Colombi, S
Colombo, LPL
Comis, B
Coulais, A
Crill, BP
Cuttaia, F
Da Silva, A
Dahle, H
Davis, RJ
de Bernardis, P
de Gasperis, G
de Rosa, A
de Zotti, G
Delabrouille, J
Democles, J
Diego, JM
Dole, H
Donzelli, S
Dore, O
Douspis, M
Dupac, X
Efstathiou, G
Ensslin, TA
Finelli, F
Flores-Cacho, I
Forni, O
Frailis, M
Franceschi, E
Frommert, M
Galeotta, S
Ganga, K
Genova-Santos, RT
Giard, M
Giraud-Heraud, Y
Gonzalez-Nuevo, J
Gorski, KM
Gregorio, A
Gruppuso, A
Hansen, FK
Harrison, D
Hernandez-Monteagudo, C
Herranz, D
Hildebrandt, SR
Hivon, E
Hobson, M
Holmes, WA
Hornstrup, A
Hovest, W
Huffenberger, KM
Hurier, G
Jaffe, TR
Jaffe, AH
Jones, WC
Juvela, M
Keihanen, E
Keskitalo, R
Khamitov, I
Kisner, TS
Kneissl, R
Knoche, J
Kunz, M
Kurki-Suonio, H
Laheenmaki, A
Lamarre, JM
Lasenby, A
Lawrence, CR
Le Jeune, M
Leonardi, R
Lilje, PB
Linden-Vornle, M
Lopez-Caniego, M
Lubin, PM
Luzzi, G
Macias-Perez, JF
MacTavish, CJ
Maffei, B
Maino, D
Mandolesi, N
Maris, M
Marleau, F
Marshall, DJ
Martinez-Gonzalez, E
Masi, S
Massardi, M
Matarrese, S
Mazzotta, P
Mei, S
Melchiorri, A
Melin, JB
Mendes, L
Mennella, A
Mitra, S
Miville-Deschenes, MA
Moneti, A
Montier, L
Morgante, G
Mortlock, D
Munshi, D
Murphy, JA
Naselsky, P
Nati, F
Natoli, P
Norgaard-Nielsen, HU
Noviello, F
Novikov, D
Novikov, I
Osborne, S
Oxborrow, CA
Pajot, F
Paoletti, D
Perotto, L
Perrotta, F
Piacentini, F
Piat, M
Pierpaoli, E
Piffaretti, R
Plaszczynski, S
Pointecouteau, E
Polenta, G
Popa, L
Poutanen, T
Pratt, GW
Prunet, S
Puget, JL
Rachen, JP
Rebolo, R
Reinecke, M
Remazeilles, M
Renault, C
Ricciardi, S
Ristorcelli, I
Rocha, G
Roman, M
Rosset, C
Rossetti, M
Rubino-Martin, JA
Rusholme, B
Sandri, M
Savini, G
Scott, D
Spencer, L
Starck, JL
Stolyarov, V
Sudiwala, R
Sunyaev, R
Sutton, D
Suur-Uski, AS
Sygnet, JF
Tauber, JA
Terenzi, L
Toffolatti, L
Tomasi, M
Tristram, M
Valenziano, L
Van Tent, B
Vielva, P
Villa, F
Vittorio, N
Wade, LA
Wandelt, BD
Wang, W
Welikala, N
Weller, J
White, SDM
White, M
Yvon, D
Zacchei, A
Zonca, A
AF Ade, P. A. R.
Aghanim, N.
Arnaud, M.
Ashdown, M.
Atrio-Barandela, F.
Aumont, J.
Baccigalupi, C.
Balbi, A.
Banday, A. J.
Barreiro, R. B.
Barrena, R.
Bartlett, J. G.
Battaner, E.
Benabed, K.
Bernard, J. -P.
Bersanelli, M.
Bikmaev, I.
Bock, J. J.
Boehringer, H.
Bonaldi, A.
Bond, J. R.
Borrill, J.
Bouchet, F. R.
Bourdin, H.
Burenin, R.
Burigana, C.
Butler, R. C.
Cabella, P.
Chamballu, A.
Chary, R. -R.
Chiang, L. -Y
Chon, G.
Christensen, P. R.
Clements, D. L.
Colafrancesco, S.
Colombi, S.
Colombo, L. P. L.
Comis, B.
Coulais, A.
Crill, B. P.
Cuttaia, F.
Da Silva, A.
Dahle, H.
Davis, R. J.
de Bernardis, P.
de Gasperis, G.
de Rosa, A.
de Zotti, G.
Delabrouille, J.
Democles, J.
Diego, J. M.
Dole, H.
Donzelli, S.
Dore, O.
Douspis, M.
Dupac, X.
Efstathiou, G.
Ensslin, T. A.
Finelli, F.
Flores-Cacho, I.
Forni, O.
Frailis, M.
Franceschi, E.
Frommert, M.
Galeotta, S.
Ganga, K.
Genova-Santos, R. T.
Giard, M.
Giraud-Heraud, Y.
Gonzalez-Nuevo, J.
Gorski, K. M.
Gregorio, A.
Gruppuso, A.
Hansen, F. K.
Harrison, D.
Hernandez-Monteagudo, C.
Herranz, D.
Hildebrandt, S. R.
Hivon, E.
Hobson, M.
Holmes, W. A.
Hornstrup, A.
Hovest, W.
Huffenberger, K. M.
Hurier, G.
Jaffe, T. R.
Jaffe, A. H.
Jones, W. C.
Juvela, M.
Keihanen, E.
Keskitalo, R.
Khamitov, I.
Kisner, T. S.
Kneissl, R.
Knoche, J.
Kunz, M.
Kurki-Suonio, H.
Laheenmaki, A.
Lamarre, J. -M.
Lasenby, A.
Lawrence, C. R.
Le Jeune, M.
Leonardi, R.
Lilje, P. B.
Linden-Vornle, M.
Lopez-Caniego, M.
Lubin, P. M.
Luzzi, G.
Macias-Perez, J. F.
MacTavish, C. J.
Maffei, B.
Maino, D.
Mandolesi, N.
Maris, M.
Marleau, F.
Marshall, D. J.
Martinez-Gonzalez, E.
Masi, S.
Massardi, M.
Matarrese, S.
Mazzotta, P.
Mei, S.
Melchiorri, A.
Melin, J. -B.
Mendes, L.
Mennella, A.
Mitra, S.
Miville-Deschenes, M. -A.
Moneti, A.
Montier, L.
Morgante, G.
Mortlock, D.
Munshi, D.
Murphy, J. A.
Naselsky, P.
Nati, F.
Natoli, P.
Norgaard-Nielsen, H. U.
Noviello, F.
Novikov, D.
Novikov, I.
Osborne, S.
Oxborrow, C. A.
Pajot, F.
Paoletti, D.
Perotto, L.
Perrotta, F.
Piacentini, F.
Piat, M.
Pierpaoli, E.
Piffaretti, R.
Plaszczynski, S.
Pointecouteau, E.
Polenta, G.
Popa, L.
Poutanen, T.
Pratt, G. W.
Prunet, S.
Puget, J. -L.
Rachen, J. P.
Rebolo, R.
Reinecke, M.
Remazeilles, M.
Renault, C.
Ricciardi, S.
Ristorcelli, I.
Rocha, G.
Roman, M.
Rosset, C.
Rossetti, M.
Rubino-Martin, J. A.
Rusholme, B.
Sandri, M.
Savini, G.
Scott, D.
Spencer, L.
Starck, J. -L.
Stolyarov, V.
Sudiwala, R.
Sunyaev, R.
Sutton, D.
Suur-Uski, A. -S.
Sygnet, J. -F.
Tauber, J. A.
Terenzi, L.
Toffolatti, L.
Tomasi, M.
Tristram, M.
Valenziano, L.
Van Tent, B.
Vielva, P.
Villa, F.
Vittorio, N.
Wade, L. A.
Wandelt, B. D.
Wang, W.
Welikala, N.
Weller, J.
White, S. D. M.
White, M.
Yvon, D.
Zacchei, A.
Zonca, A.
CA Planck Collaboration
TI Planck intermediate results XI. The gas content of dark matter halos:
the Sunyaev-Zeldovich-stellar mass relation for locally brightest
galaxies
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE cosmology: observations; cosmic background radiation; large-scale
structure of Universe; galaxies: clusters: general
ID ACTIVE GALACTIC NUCLEI; SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY;
PRE-LAUNCH STATUS; BLACK-HOLES; INTRACLUSTER MEDIUM; SCALING RELATIONS;
COOLING FLOWS; AGN FEEDBACK; CLUSTERS
AB We present the scaling relation between Sunyaev-Zeldovich (SZ) signal and stellar mass for almost 260,000 locally brightest galaxies (LBGs) selected from the Sloan Digital Sky Survey (SDSS). These are predominantly the central galaxies of their dark matter halos. We calibrate the stellar-to-halo mass conversion using realistic mock catalogues based on the Millennium Simulation. Applying a multi-frequency matched filter to the Planck data for each LBG, and averaging the results in bins of stellar mass, we measure the mean SZ signal down to M-* similar to 2 x 10(11) M-circle dot, with a clear indication of signal at even lower stellar mass. We derive the scaling relation between SZ signal and halo mass by assigning halo properties from our mock catalogues to the real LBGs and simulating the Planck observation process. This relation shows no evidence for deviation from a power law over a halo mass range extending from rich clusters down to M-500 similar to 2 x 10(13) M-circle dot, and there is a clear indication of signal down to M-500 similar to 4 x 10(12) M-circle dot. Planck's SZ detections in such low-mass halos imply that about a quarter of all baryons have now been seen in the form of hot halo gas, and that this gas must be less concentrated than the dark matter in such halos in order to remain consistent with X-ray observations. At the high-mass end, the measured SZ signal is 20 % lower than found from observations of X-ray clusters, a difference consistent with the magnitude of Malmquist bias effects that were previously estimated for the X-ray sample.
C1 [Bartlett, J. G.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Le Jeune, M.; Piat, M.; Remazeilles, M.; Roman, M.; Rosset, C.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, APC,CNRS,IN2P3,CEA lrfu, F-75205 Paris 13, France.
[Laheenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland.
[Bikmaev, I.] Acad Sci Tatarstan, Kazan 420111, Russia.
[Kunz, M.] African Inst Math Sci, Cape Town, South Africa.
[Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy.
[Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy.
[Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
[Kneissl, R.] ALMA Santiago Cent Off, Santiago 0355, Chile.
[Bond, J. R.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Banday, A. J.; Bernard, J. -P.; Flores-Cacho, I.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse, France.
[Bock, J. J.; Crill, B. P.; Dore, O.; Hildebrandt, S. R.; Mei, S.; Rocha, G.] CALTECH, Pasadena, CA 91125 USA.
[Da Silva, A.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Hernandez-Monteagudo, C.] CEFCA, Teruel 44001, Spain.
[Borrill, J.; Keskitalo, R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Rebolo, R.] CSIC, Madrid, Spain.
[Chamballu, A.; Melin, J. -B.; Piffaretti, R.; Yvon, D.] CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France.
[Hornstrup, A.; Linden-Vornle, M.; Norgaard-Nielsen, H. U.; Oxborrow, C. A.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Frommert, M.; Kunz, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva, Switzerland.
[Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain.
[Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain.
[Bikmaev, I.; Khamitov, I.] Kazan Fed Univ, Dept Astron & Geodesy, Kazan 420008, Russia.
[Rachen, J. P.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
[Keskitalo, R.] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA.
[Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
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[Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Matarrese, S.] Univ Padua, Dipartimento Fis Astron G Galilei, I-35131 Padua, Italy.
[Burigana, C.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy.
[de Bernardis, P.; Masi, S.; Melchiorri, A.; Nati, F.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Bersanelli, M.; Maino, D.; Mennella, A.; Rossetti, M.] Univ Milan, Dipartimento Fis, Milan, Italy.
[Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy.
[Balbi, A.; Bourdin, H.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy.
[Cabella, P.] Univ Roma Tor Vergata, Dipartimento Matemat, I-00133 Rome, Italy.
[Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark.
[Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, Tenerife, Spain.
[Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile.
[Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, Planck Sci Off, Madrid, Spain.
[Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands.
[Mei, S.] Observ Paris, GEPI, Sect Meudon, F-92195 Meudon, France.
[Kurki-Suonio, H.; Laheenmaki, A.; Poutanen, T.; Suur-Uski, A. -S.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland.
[de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy.
[Colafrancesco, S.; Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Frailis, M.; Galeotta, S.; Gregorio, A.; Maris, M.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Massardi, M.] CNR, Ist Radioastron, INAF, I-40129 Bologna, Italy.
[Burigana, C.; Butler, R. C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] IASF Bologna, INAF, Bologna, Italy.
[Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] IASF Milano, INAF, Milan, Italy.
[Finelli, F.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy.
[Melchiorri, A.] Univ Roma Sapienza, INFN, Sez Roma 1, I-00185 Rome, Italy.
[Mitra, S.] IUCAA, Pune 411007, Maharashtra, India.
[Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Chary, R. -R.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Dole, H.] Inst Univ France, F-75005 Paris, France.
[Aghanim, N.; Aumont, J.; Chamballu, A.; Dole, H.; Douspis, M.; Kunz, M.; Miville-Deschenes, M. -A.; Pajot, F.; Puget, J. -L.; Remazeilles, M.; Welikala, N.] Univ Paris Sud 11, CNRS, Inst Astrophys Spatiale, UMR 8617, Orsay, France.
[Benabed, K.; Bouchet, F. R.; Colombi, S.; Hivon, E.; Moneti, A.; Prunet, S.; Ricciardi, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Popa, L.] Inst Space Sci, Bucharest, Romania.
[Marleau, F.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria.
[Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Efstathiou, G.; Harrison, D.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Dahle, H.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway.
[Barrena, R.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain.
[Barreiro, R. B.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain.
[Bartlett, J. G.; Bock, J. J.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Rocha, G.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bonaldi, A.; Davis, R. J.; Maffei, B.; Noviello, F.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Ashdown, M.; Harrison, D.; Lasenby, A.; MacTavish, C. J.; Stolyarov, V.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
[Luzzi, G.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS, IN2P3, LAL, F-91405 Orsay, France.
[Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France.
[Arnaud, M.; Chamballu, A.; Democles, J.; Marshall, D. J.; Piffaretti, R.; Pratt, G. W.; Starck, J. -L.] CEA Saclay, Univ Paris Diderot, CNRS, CEA,DSM,IRFU,Serv Astrophys,Lab AIM, F-91191 Gif Sur Yvette, France.
[Comis, B.; Hurier, G.; Macias-Perez, J. F.; Perotto, L.; Renault, C.] Univ Joseph Fourier Grenoble I, Inst Natl Polytech Grenoble, CNRS IN2P3, Lab Phys Subatom & Cosmol, F-38026 Grenoble, France.
[Van Tent, B.] Univ Paris Sud 11, Phys Theor Lab, F-91405 Orsay, France.
[Van Tent, B.] CNRS, F-91405 Orsay, France.
[Kisner, T. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Rachen, J. P.; Reinecke, M.; Sunyaev, R.; Wang, W.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Boehringer, H.; Chon, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland.
[Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Savini, G.] UCL, Opt Sci Lab, London, England.
[Baccigalupi, C.; de Zotti, G.; Gonzalez-Nuevo, J.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Ade, P. A. R.; Munshi, D.; Spencer, L.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales.
[Burenin, R.; Sunyaev, R.] Space Res Inst IKI, Moscow, Russia.
[Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Zelenchukskiy, Russia.
[Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Khamitov, I.] TUBITAK Natl Observ, TR-07058 Antalya, Turkey.
[Benabed, K.; Bouchet, F. R.; Colombi, S.; Hivon, E.; Prunet, S.; Ricciardi, S.; Wandelt, B. D.] Univ Paris 06, UMR 7095, F-75014 Paris, France.
[Mei, S.] Univ Denis Diderot Paris 7, F-75205 Paris 13, France.
[Banday, A. J.; Flores-Cacho, I.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France.
[Weller, J.] Univ Munich, Univ Observ, D-81679 Munich, Germany.
[Battaner, E.] Univ Granada, Fac Ciencias, Dept Fisica Teor & Cosmos, Granada, Spain.
[Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Rubino-Martin, JA (reprint author), Inst Astrofis Canarias, C-Via Lactea S-N, Tenerife, Spain.
EM jalberto@iac.es
RI Battaner, Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon,
Dominique/D-2280-2015; Lopez-Caniego, Marcos/M-4695-2013; Da Silva,
Antonio/A-2693-2010; Bouchet, Francois/B-5202-2014; Martinez-Gonzalez,
Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; White,
Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015; Vielva,
Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; Herranz,
Diego/K-9143-2014; Butler, Reginald/N-4647-2015; Remazeilles,
Mathieu/N-1793-2015; Novikov, Dmitry/P-1807-2015; Kurki-Suonio,
Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov,
Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati,
Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini,
Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov,
Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016;
OI Barreiro, Rita Belen/0000-0002-6139-4272; Da Silva,
Antonio/0000-0002-6385-1609; Martinez-Gonzalez,
Enrique/0000-0002-0179-8590; Gonzalez-Nuevo,
Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070;
Gruppuso, Alessandro/0000-0001-9272-5292; Vielva,
Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386;
Herranz, Diego/0000-0003-4540-1417; Hivon, Eric/0000-0003-1880-2733;
Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147;
Savini, Giorgio/0000-0003-4449-9416; Pierpaoli,
Elena/0000-0002-7957-8993; Ricciardi, Sara/0000-0002-3807-4043; Villa,
Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck,
Jean-Luc/0000-0003-2177-7794; Hurier, Guillaume/0000-0002-1215-0706;
Zacchei, Andrea/0000-0003-0396-1192; Polenta,
Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996;
Sandri, Maura/0000-0003-4806-5375; Cuttaia,
Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099;
Burigana, Carlo/0000-0002-3005-5796; Bouchet,
Francois/0000-0002-8051-2924; Valenziano, Luca/0000-0002-1170-0104;
Galeotta, Samuele/0000-0002-3748-5115; WANDELT,
Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269;
Frailis, Marco/0000-0002-7400-2135; Weller, Jochen/0000-0002-8282-2010;
Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio,
Anna/0000-0003-4028-8785; Matarrese, Sabino/0000-0002-2573-1243; Scott,
Douglas/0000-0002-6878-9840; Masi, Silvia/0000-0001-5105-1439; de
Bernardis, Paolo/0000-0001-6547-6446; Forni,
Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412;
Remazeilles, Mathieu/0000-0001-9126-6266; Maris,
Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591;
Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi,
Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati,
Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327;
Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov,
Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748;
Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti,
Gianfranco/0000-0003-2868-2595
FU CNES; CNRS; ASI; NASA; Danish Natural Research Council; ESA;
CNRS/INSU-IN2P3-INP (France); INAF (Italy); DoE (USA); STFC; UKSA (UK);
CSIC; MICINN; JA; RES (Spain); Tekes; AoF; CSC (Finland); DLR; MPG
(Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN
(Norway); SFI (Ireland); FCT/MCTES (Portugal); PRACE (EU)
FX The authors from the consortia funded principally by CNES, CNRS, ASI,
NASA, and Danish Natural Research Council acknowledge the use of the
pipeline-running infrastructures Magique3 at Institut d'Astrophysique de
Paris (France), CPAC at Cambridge (UK), and USPDC at IPAC (USA). The
development of Planck has been supported by: ESA; CNES and
CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE
(USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration
and a list of its members, including the technical or scientific
activities in which they have been involved, can be found at
http://www.sciops.esa.int/index.php?project=planck. We acknowledge the
use of the HEALPix package (Gorski et al. 2005).
NR 81
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U1 2
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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 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2013
VL 557
AR A52
DI 10.1051/0004-6361/201220941
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 228TC
UT WOS:000325211900027
ER
PT J
AU Bethermin, M
Wang, LY
Dore, O
Lagache, G
Sargent, M
Daddi, E
Cousin, M
Aussel, H
AF Bethermin, Matthieu
Wang, Lingyu
Dore, Olivier
Lagache, Guilaine
Sargent, Mark
Daddi, Emanuele
Cousin, Morgane
Aussel, Herve
TI The redshift evolution of the distribution of star formation among dark
matter halos as seen in the infrared
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: star formation; galaxies: halos; galaxies: statistics; diffuse
radiation; dark matter; submillimeter: galaxies
ID MULTIBAND IMAGING PHOTOMETER; SUBMILLIMETER NUMBER COUNTS; ACTIVE
GALACTIC NUCLEI; SIMILAR-TO 2; LESS-THAN 2; 500 MU-M; FORMING GALAXIES;
STELLAR MASS; LUMINOSITY FUNCTION; BACKGROUND LIGHT
AB Recent studies have revealed a strong correlation between the star formation rate (SFR) and stellar mass of the majority of star-forming galaxies, the so-called star-forming main sequence. An empirical modeling approach (the 2-SFM framework) that distinguishes between the main sequence and rarer starburst galaxies is capable of reproducing most statistical properties of infrared galaxies, such as number counts, luminosity functions, and redshift distributions. In this paper, we extend this approach by establishing a connection between stellar mass and halo mass with the technique of abundance matching. Based on a few simple assumptions and a physically motivated formalism, our model successfully predicts the (cross-) power spectra of the cosmic infrared background (CIB), the cross-correlation between CIB and cosmic microwave background (CMB) lensing, and the correlation functions of bright, resolved infrared galaxies measured by Herschel, Planck, ACT, and SPT. We use this model to infer the redshift distribution of CIB-anisotropies and of the CIB x CMB lensing signal, as well as the level of correlation between CIB-anisotropies at different wavelengths. We study the link between dark matter halos and star-forming galaxies in the framework of our model. We predict that more than 90% of cosmic star formation activity occurs in halos with masses between 10(11.5) and 10(13.5) M-circle dot. If taking subsequent mass growth of halos into account, this implies that the majority of stars were initially (at z > 3) formed in the progenitors of clusters (M-h(z = 0) > 10(13.5) M-circle dot), then in groups (10(12.)5 < M-h(z = 0) < 10(13.5) M-circle dot) at 0.5 < z < 3, and finally in Milky-Way-like halos (1011.5 < M-h(z = 0) < 10(12.5) M-circle dot) at z < 0.5. At all redshifts, the dominant contribution to the SFR density stems from halos of mass similar to 10(12) M-circle dot, in which the instantaneous star formation efficiency - defined here as the ratio between SFR and baryonic accretion rate - is maximal (similar to 70%). The strong redshift-evolution of SFR in the galaxies that dominate the CIB is thus plausibly driven by increased accretion from the cosmic web onto halos of this characteristic mass scale. Material (effective spectral energy distributions, differential emissivities of halos, relations between M-h and SFR) associated to this model is available at http://irfu.cea.fr/Sap/Phocea/Page/index.php?id=537.
C1 [Bethermin, Matthieu; Sargent, Mark; Daddi, Emanuele; Aussel, Herve] Univ Paris Diderot, CEA Saclay, CNRS, CEA DSM Irfu,Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France.
[Wang, Lingyu] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Dore, Olivier] CALTECH, Pasadena, CA 91125 USA.
[Lagache, Guilaine; Cousin, Morgane] Univ Paris 11, CNRS, UMR 8617, Inst Astrophys Spatiale, F-91405 Orsay, France.
RP Bethermin, M (reprint author), Univ Paris Diderot, CEA Saclay, CNRS, CEA DSM Irfu,Lab AIM Paris Saclay, Pt Courrier 131, F-91191 Gif Sur Yvette, France.
EM matthieu.bethermin@cea.fr
RI Daddi, Emanuele/D-1649-2012;
OI Daddi, Emanuele/0000-0002-3331-9590; Bethermin,
Matthieu/0000-0002-3915-2015
FU ERC-StG UPGAL [240039, ANR-08-JCJC-0008]; ERC StG grant [DEGAS-259586];
NASA
FX We thank Steve Maddox for providing data and discussion about clustering
measurements, Marco Viero and Amir Hajian for providing data, Paolo
Serra for useful discussion, and the anonymous referee for very
constructive comments. M. B., E. D., and M. S. acknowledge the support
provided by the grants ERC-StG UPGAL 240039 and ANR-08-JCJC-0008. L. W.
acknowledges support from an ERC StG grant (DEGAS-259586). This research
was carried out in part at the Jet Propulsion Laboratory, run by the
California Institute of Technology under a contract from NASA.
NR 114
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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 SEP
PY 2013
VL 557
AR A66
DI 10.1051/0004-6361/201321688
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 228TC
UT WOS:000325211900094
ER
PT J
AU Correia, S
Duchene, G
Reipurth, B
Zinnecker, H
Daemgen, S
Petr-Gotzens, MG
Kohler, R
Ratzka, T
Aspin, C
Konopacky, QM
Ghez, AM
AF Correia, S.
Duchene, G.
Reipurth, B.
Zinnecker, H.
Daemgen, S.
Petr-Gotzens, M. G.
Koehler, R.
Ratzka, Th.
Aspin, C.
Konopacky, Q. M.
Ghez, A. M.
TI Stellar and circumstellar properties of visual binaries in the Orion
Nebula Cluster
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: pre-main sequence; binaries: close; techniques: high angular
resolution
ID T-TAURI STARS; MAIN-SEQUENCE BINARIES; LOW-MASS STARS;
HUBBLE-SPACE-TELESCOPE; SOLAR-TYPE STARS; H-R DIAGRAM; SPECTROSCOPIC
SURVEY; RESOLUTION SPECTRA; TRAPEZIUM CLUSTER; PLANET FORMATION
AB Context. Our general understanding of multiple star and planet formation is primarily based on observations of young multiple systems in low density regions like Tau-Aur and Oph. Since many, if not most, of the stars are born in clusters, observational constraints from young binaries in those environments are fundamental for understanding both the formation of multiple systems and planets in multiple systems throughout the Galaxy.
Aims. We build upon the largest survey for young binaries in the Orion Nebula Cluster (ONC), which is based on Hubble Space Telescope observations to derive both stellar and circumstellar properties of newborn binary systems in this cluster environment.
Methods. We present adaptive optics spatially-resolved JHKL'-band photometry and K-band R similar to 5000 spectra for a sample of eight ONC binary systems from this database. We characterize the stellar properties of binary components and obtain a census of protoplanetary disks through K - L' color excess. For a combined sample of ONC binaries including 7 additional systems with NIR spectroscopy from the literature, we derive mass ratio and relative age distributions. We compare the stellar and circumstellar properties of binaries in ONC with those in Tau-Aur and Oph from samples of binaries with stellar properties derived for each component from spectra and/or visual photometry and with a disk census obtained through K - L color excess.
Results. The mass ratio distribution of ONC binaries is found to be indistinguishable from that of Tau-Aur and, to some extent, to that of Oph in the separation range 85-560 AU and for primary mass in the range 0.15 to 0.8 M-circle dot. A trend toward a lower mass ratio with larger separation is suggested in ONC binaries, which is not seen in Tau-Aur binaries. The components of ONC binaries are found to be significantly more coeval than the overall ONC population and as coeval as components of binaries in Tau-Aur and Oph. There is a hint of a larger fraction of mixed pairs, i.e. systems with a disk around only one component, in wide ONC binaries in comparison to wide binaries in Tau-Aur and Oph within the same primary mass range that could be caused by hierarchical triples. The mass ratio distributions of mixed and unmixed pairs in the overall population of T Tauri binaries are shown to be different. Some of these trends require confirmation with observations of a larger sample of binary systems.
C1 [Correia, S.] Leibniz Inst Astrophys Potsdam, D-14482 Potsdam, Germany.
[Correia, S.] Univ Hawaii, Inst Astron, Pukalani, HI 96768 USA.
[Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Duchene, G.] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys Grenoble, UMR 5274, F-38041 Grenoble, France.
[Reipurth, B.; Aspin, C.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Reipurth, B.] Univ Stuttgart, NASA Astrobiol Inst, D-70569 Stuttgart, Germany.
[Zinnecker, H.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
[Zinnecker, H.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Daemgen, S.; Petr-Gotzens, M. G.] European So Observ, D-85748 Garching, Germany.
[Daemgen, S.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Koehler, R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Koehler, R.] Heidelberg Univ, Zentrum Astron, Landessternwarte, D-69117 Heidelberg, Germany.
[Ratzka, Th.] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Konopacky, Q. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Ghez, A. M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Ghez, A. M.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
RP Correia, S (reprint author), Leibniz Inst Astrophys Potsdam, Sternwarte 16, D-14482 Potsdam, Germany.
EM sergeco@gmail.com
OI Ratzka, Thorsten/0000-0001-9557-8232
FU National Aeronautics and Space Administration through the NASA
Astrobiology Institute through the Office of Space Science [NNA09DA77A]
FX We thank the referee for detailed and helpful comments on this paper.
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
material is based upon work supported by the National Aeronautics and
Space Administration through the NASA Astrobiology Institute under
Cooperative Agreement No. NNA09DA77A issued through the Office of Space
Science. This research made use of data products from the Two Micron All
Sky Survey and of the SIMBAD database, operated at CDS, Strasbourg,
France.
NR 85
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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 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2013
VL 557
AR A63
DI 10.1051/0004-6361/201220681
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 228TC
UT WOS:000325211900024
ER
PT J
AU Dartois, E
Ding, JJ
de Barros, ALF
Boduch, P
Brunetto, R
Chabot, M
Domaracka, A
Godard, M
Lv, XY
Guaman, CFM
Pino, T
Rothard, H
da Silveira, EF
Thomas, JC
AF Dartois, E.
Ding, J. J.
de Barros, A. L. F.
Boduch, P.
Brunetto, R.
Chabot, M.
Domaracka, A.
Godard, M.
Lv, X. Y.
Guaman, C. F. Mejia
Pino, T.
Rothard, H.
da Silveira, E. F.
Thomas, J. C.
TI Swift heavy ion irradiation of water ice from MeV to GeV energies
Approaching true cosmic ray compaction
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE cosmic rays; dust, extinction; ISM: molecules; line: profiles; molecular
processes
ID CROSS-SECTIONS; AMORPHOUS ICE; MOLECULAR CLOUDS; IONIZATION RATE; SOLID
WATER; HYDROGEN; SPECTRA; MORPHOLOGY; SURFACES; PROTONS
AB Context. Cosmic ray ion irradiation affects the chemical composition of and triggers physical changes in interstellar ice mantles in space. One of the primary structural changes induced is the loss of porosity, and the mantles evolve toward a more compact amorphous state. Previously, ice compaction was monitored at low to moderate ion energies. The existence of a compaction threshold in stopping power has been suggested.
Aims. In this article we experimentally study the effect of heavy ion irradiation at energies closer to true cosmic rays. This minimises extrapolation and allows a regime where electronic interaction always dominates to be explored, providing the ice compaction cross section over a wide range of electronic stopping power.
Methods. High-energy ion irradiations provided by the GANIL accelerator, from the MeV up to the GeV range, are combined with in-situ infrared spectroscopy monitoring of ice mantles. We follow the IR spectral evolution of the ice as a function of increasing fluence (induced compaction of the initial microporous amorphous ice into a more compact amorphous phase). We use the number of OH dangling bonds of the water molecule, i.e. pending OH bonds not engaged in a hydrogen bond in the initially porous ice structure as a probe of the phase transition. These high-energy experiments are combined with lower energy experiments using light ions (H, He) from other facilities in Catania, Italy, and Washington, USA.
Results. We evaluated the cross section for the disappearance of OH dangling bonds as a function of electronic stopping power. A cross-section law in a large energy range that includes data from different ice deposition setups is established. The relevant phase structuring time scale for the ice network is compared to interstellar chemical time scales using an astrophysical model.
Conclusions. The presence of a threshold in compaction at low stopping power suggested in some previous works seems not to be confirmed for the high-energy cosmic rays encountered in interstellar space. Ice mantle porosity or pending bonds monitored by the OH dangling bonds is removed efficiently by cosmic rays. As a consequence, this considerably reduces the specific surface area available for surface chemical reactions.
C1 [Dartois, E.; Brunetto, R.; Godard, M.] CNRS INSU, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France.
[Dartois, E.; Brunetto, R.; Godard, M.] Univ Paris 11, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France.
[Ding, J. J.; Boduch, P.; Domaracka, A.; Lv, X. Y.; Rothard, H.] Univ Caen Basse Normandie, Ctr Rech Ions Mat & Photon, CIMAP CIRIL Ganil, CEA,CNRS,ENSICAEN, F-14070 Caen 5, France.
[de Barros, A. L. F.] Ctr Fed Educ Tecnol Celso Suckow Fonseca, Dept Phys, BR-20271110 Rio De Janeiro, RJ, Brazil.
[Chabot, M.] CNRS, IN2P3, Inst Phys Nucl Orsay, UMR8608, F-91406 Orsay, France.
[Chabot, M.] Univ Paris 11, Inst Phys Nucl Orsay, UMR8608, CNRS IN2P3, F-91406 Orsay, France.
[Godard, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Guaman, C. F. Mejia; da Silveira, E. F.] Pontificia Univ Catolica Rio de Janeiro, Dept Phys, BR-22451900 Rio De Janeiro, RJ, Brazil.
[Pino, T.] Univ Paris 11, CNRS, Inst Sci Mol Orsay, UMR 8214, F-91405 Orsay, France.
[Thomas, J. C.] CEA DSM CNRS IN2P3, Grand Accelerateur Natl Ions Lourds, F-14076 Caen 5, France.
RP Dartois, E (reprint author), CNRS INSU, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France.
EM emmanuel.dartois@ias.u-psud.fr
RI Godard, Marie/H-6451-2011
OI Godard, Marie/0000-0002-7276-4021
FU French INSU-CNRS program Physique et Chimie du Milieu Interstellaire
(PCMI)
FX We would like to warmly thank G. Strazzulla and M. E. Palumbo for not
only sending us data used in this article, but also for fruitful
discussions. We would like to thank Marla Moore for digging into several
years old data to allow for another point in this study. The authors
would like to cordially thank the anonymous referee for the comments
improving the scientific content of the article, as well as the edition
team for suggestions on the language and structure of the manuscript.
The experiments were performed at the Grand Accelerateur National d'Ions
Lourds (GANIL) Caen, France. We would like to thank the LISE staff and
in particular Omar Kamalou. Part of the equipment used in this work has
been financed by the French INSU-CNRS program Physique et Chimie du
Milieu Interstellaire (PCMI).
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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 SEP
PY 2013
VL 557
AR A97
DI 10.1051/0004-6361/201321636
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 228TC
UT WOS:000325211900086
ER
PT J
AU Marshall, JP
Krivov, AV
del Burgo, C
Eiroa, C
Mora, A
Montesinos, B
Ertel, S
Bryden, G
Liseau, R
Augereau, JC
Bayo, A
Danchi, W
Lohne, T
Maldonado, J
Pilbratt, GL
Stapelfeldt, K
Thebault, P
White, GJ
Wolf, S
AF Marshall, J. P.
Krivov, A. V.
del Burgo, C.
Eiroa, C.
Mora, A.
Montesinos, B.
Ertel, S.
Bryden, G.
Liseau, R.
Augereau, J. -C.
Bayo, A.
Danchi, W.
Loehne, T.
Maldonado, J.
Pilbratt, G. L.
Stapelfeldt, K.
Thebault, P.
White, G. J.
Wolf, S.
TI Herschel observations of the debris disc around HIP 92043
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Infrared: stars; circumstellar matter; Stars: individual: HIP 92043 (110
Her, HD 173667)
ID ATMOSPHERIC PARAMETERS; BOLOMETRIC CORRECTIONS; SPIRE INSTRUMENT; HD
207129; STARS; DUST; SEARCH; COLD; PERFORMANCE; ROTATION
AB Context. Typical debris discs are composed of particles ranging from several micron sized dust grains to km sized asteroidal bodies, and their infrared emission peaks at wavelengths 60-100 mu m. Recent Herschel DUNES observations have identified several debris discs around nearby Sun-like stars (F, G and K spectral type) with significant excess emission only at 160 mu m.
Aims. We observed HIP 92043 (110 Her, HD 173667) at far-infrared and sub-millimetre wavelengths with Herschel PACS and SPIRE. Identification of the presence of excess emission from HIP 92043 and the origin and physical properties of any excess was undertaken through analysis of its spectral energy distribution (SED) and the PACS images.
Methods. The PACS and SPIRE images were produced using the HIPE photProject map maker routine. Fluxes were measured using aperture photometry. A stellar photosphere model was scaled to optical and near infrared photometry and subtracted from the far-infared and sub-mm fluxes to determine the presence of excess emission. Source radial profiles were fitted using a 2D Gaussian and compared to a PSF model based on Herschel observations of alpha Boo to check for extended emission.
Results. Clear excess emission from HIP 92043 was observed at 70 and 100 mu m. Marginal excess was observed at 160 and 250 mu m. Analysis of the images reveals that the source is extended at 160 mu m. A fit to the source SED is inconsistent with a photosphere and single temperature black body.
Conclusions. The excess emission from HIP 92043 is consistent with the presence of an unresolved circumstellar debris disc at 70 and 100 mu m, with low probability of background contamination. The extended 160 mu m emission may be interpreted as an additional cold component to the debris disc or as the result of background contamination along the line of sight. The nature of the 160 mu m excess cannot be determined absolutely from the available data, but we favour a debris disc interpretation, drawing parallels with previously identified cold disc sources in the DUNES sample.
C1 [Marshall, J. P.; Eiroa, C.; Maldonado, J.] Univ Autonoma Madrid, Dept Fis Teor, Fac Ciencias, E-28049 Madrid, Spain.
[Krivov, A. V.; Loehne, T.] Univ Jena, Inst Astrophys, D-07745 Jena, Germany.
[Krivov, A. V.; Loehne, T.] Univ Jena, Univ Sternwarte, D-07745 Jena, Germany.
[del Burgo, C.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Pue, Mexico.
[del Burgo, C.] UNINOVA CA3, P-2825149 Caparica, Portugal.
[Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain.
[Montesinos, B.] Ctr Astrobiol CAB CSIC INTA, Dept Astrophys, Madrid 28691, Spain.
[Ertel, S.; Augereau, J. -C.; Thebault, P.] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys Grenoble, UMR 5274, F-38041 Grenoble, France.
[Ertel, S.; Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany.
[Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Liseau, R.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden.
[Bayo, A.] European Space Observ, Santiago 19, Chile.
[Danchi, W.; Stapelfeldt, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pilbratt, G. L.] ESA, Res & Sci Support Dept, ESTEC SRE SA, NL-2201 AZ Noordwijk, Netherlands.
[Thebault, P.] LESIA, Observ Paris, F-92195 Meudon, France.
[White, G. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[White, G. J.] Rutherford Appleton Lab, Chilton OX11 0QX, England.
RP Marshall, JP (reprint author), Univ Autonoma Madrid, Dept Fis Teor, Fac Ciencias, E-28049 Madrid, Spain.
EM jonathan.marshall@uam.es
RI Montesinos, Benjamin/C-3493-2017;
OI Montesinos, Benjamin/0000-0002-7982-2095; Marshall,
Jonathan/0000-0001-6208-1801
FU Spanish MICINN [AYA 2008/02156]; FCT-Portugal [PEst-OE/EEI/UI0066/201];
DFG [WO857/7-1, Lo 1715/1-1, Kr 2164/10-1]; French Research Agency (ANR)
[ANR-2010 BLAN-0505-01]; Marie Curie Actions of the European Commission
(FP7-COFUND); [AYA 2008/01727]; [AYA 2011/26202]
FX The authors would like to collectively thank the Herschel Helpdesk and
PACS data reduction teams for their assistance in the interpretation of
the data. C. E., J.M., and J.P.M. are partly supported by Spanish grant
AYA 2008/01727 and AYA 2011/26202. The DUNES VO tool has been developed
in the framework of the Spanish Virtual Observatory project supported by
the Spanish MICINN through grant AYA 2008/02156. The system is
maintained by the Data Archive Unit of the CAB (CSIC-INTA). C.d.B. was
partly funded by the FCT-Portugal through the project
PEst-OE/EEI/UI0066/201. S. E. is grateful for financial support from DFG
under contract WO857/7-1 and from the French Research Agency (ANR) for
financial support through contract ANR-2010 BLAN-0505-01 (EXOZODI). T.
L. and A. V. K. are partly supported by DFG grants Lo 1715/1-1 and Kr
2164/10-1. The work of A. B. was co-funded under the Marie Curie Actions
of the European Commission (FP7-COFUND).
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2013
VL 557
AR A58
DI 10.1051/0004-6361/201218976
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 228TC
UT WOS:000325211900005
ER
PT J
AU Schnulle, K
Pott, JU
Rix, HW
Decarli, R
Peterson, BM
Vacca, W
AF Schnuelle, K.
Pott, J. -U.
Rix, H. -W.
Decarli, R.
Peterson, B. M.
Vacca, W.
TI Dust physics in the nucleus of NGC 4151
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: nuclei; galaxies: Seyfert; infrared:
galaxies; galaxies: individual: NGC 4151
ID ACTIVE GALACTIC NUCLEI; HOT DUST; QUASARS; TORUS; SPECTROGRAPH;
GALAXIES; SPECTRA; VARIABILITY; EMISSION; NGC-4151
AB The unified model of active galactic nuclei (AGNs) presumes the existence of a so-called dusty torus around the outer edge of the broad-line region. Despite the solid observational evidence for the existence of dust around AGNs and our growing information on the characteristic scales of these obscuring tori, the origin of this dust and its morphology are not yet well understood.
Using dust reverberation mapping, we monitor the effects of AGN continuum variability to determine the temperature and covering factor of the circumnuclear dust, in order to constrain the physical conditions for dust survival and formation in the radiation field of the AGN. Multi-band photometry observations in the z, Y, J, H, and K bands were carried out on the nucleus of the prototypical Seyfert 1 galaxy NGC 4151 over six epochs from 2010 January to June, supported by spectroscopic observations, in order to investigate the response of the hot dust to varying accretion disk emission.
Our data confirm that most of the hot dust reacts to increased radiation from the central source with a delayed brightening of similar to 50 days. In accretion disk brightening, we see no signatures of dust destruction in our data. The innermost dust appears to increase in temperature rather than sublimate, suggesting that it is cooler than sublimation temperature and located beyond the current sublimation radius. We characterize the dust geometry by interpreting the wavelength-dependent reverberation response with a simplified torus model, pointing to a static radially extended distribution of the central (similar to 0.1 pc) hot dust.
C1 [Schnuelle, K.; Pott, J. -U.; Rix, H. -W.; Decarli, R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Peterson, B. M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Vacca, W.] NASA, SOFIA, Univ Space Res Assoc, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Schnulle, K (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM schnuelle@mpia.de
FU IMPRS for Astronomy & Cosmic Physics at the University of Heidelberg; US
NSF [AST-1008882]
FX We are very thankful to the anonymous referee for significantly
improving this manuscript. We thank R. van Boekel for providing a
database of main sequence star atmospheres. K. S. acknowledges support
by "IMPRS for Astronomy & Cosmic Physics at the University of
Heidelberg". B. M. P. is grateful for the support of the US NSF through
grant AST-1008882.
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2013
VL 557
AR L13
DI 10.1051/0004-6361/201321802
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 228TC
UT WOS:000325211900113
ER
PT J
AU Snodgrass, C
Tubiana, C
Bramich, DM
Meech, K
Boehnhardt, H
Barrera, L
AF Snodgrass, C.
Tubiana, C.
Bramich, D. M.
Meech, K.
Boehnhardt, H.
Barrera, L.
TI Beginning of activity in 67P/Churyumov-Gerasimenko and predictions for
2014-2015
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE comets: individual: 67P/Churyumov-Gerasimenko
ID NARROW-BAND PHOTOMETRY; JUPITER-FAMILY COMETS; SPACE-TELESCOPE
OBSERVATIONS; DIFFERENCE IMAGE-ANALYSIS; ROSETTA MISSION TARGET;
HELIOCENTRIC DISTANCE; OPTICAL OBSERVATIONS; ENSEMBLE PROPERTIES;
PRODUCTION-RATES; COMA MORPHOLOGY
AB Context. Comet 67P/Churyumov-Gerasimenko was selected in 2003 as the new target of the Rosetta mission. It has since been the subject of a detailed campaign of observations to characterise its nucleus and activity.
Aims. We present previously unpublished data taken around the start of activity of the comet in 2007/8, before its last perihelion passage. We constrain the time of the start of activity, and combine this with other data taken throughout the comet's orbit to make predictions for its likely behaviour during 2014/5 while Rosetta is operating.
Methods. A considerable difficulty in observing 67P during the past years has been its position against crowded fields towards the Galactic centre for much of the time. The 2007/8 data presented here were particularly difficult, and the comet will once again be badly placed for Earth-based observations in 2014/5. We make use of the difference image analysis technique, which is commonly used in variable star and exoplanet research, to remove background sources and extract images of the comet. In addition, we reprocess a large quantity of archival images of 67P covering its full orbit, to produce a heliocentric lightcurve. By using consistent reduction, measurement and calibration techniques we generate a remarkably clean lightcurve, which can be used to measure a brightness-distance relationship and to predict the future brightness of the comet.
Results. We determine that the comet was active around November 2007, at a pre-perihelion distance from the Sun of 4.3 AU. The comet will reach this distance, and probably become active again, in March 2014. We find that the dust brightness can be well described by Af rho proportional to r(-3.2) pre-perihelion and proportional to r(-3.4) post-perihelion, and that the comet has a higher dust-to-gas ratio than average, with log(Af rho/Q(H2O)) = -24.94 +/- 0.22 cm s molecule(-1) at r < 2 AU. A model fit to the photometric data suggests that only a small fraction (1.4%) of the surface is active.
C1 [Snodgrass, C.; Tubiana, C.; Boehnhardt, H.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Bramich, D. M.] European So Observ, D-85748 Garching, Germany.
[Meech, K.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Meech, K.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
[Barrera, L.] Univ Metropolitana Ciencias Educ, Santiago 832000, Chile.
RP Snodgrass, C (reprint author), Max Planck Inst Solar Syst Res, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany.
EM snodgrass@mps.mpg.de
OI Snodgrass, Colin/0000-0001-9328-2905
FU European Union [268421]; ESO; NASA [NNX13A151G, NNA09DA77A]; Canadian
Space Agency; Robert Martin Ayers Sciences Fund; Alfred P. Sloan
Foundation; National Science Foundation; US Department of Energy Office
of Science; University of Arizona; Brazilian Participation Group;
Brookhaven National Laboratory; University of Cambridge; 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 made extensive use of the ESO archive, and wish to thank the staff at
ESO Headquarters in Garching who maintain this facility. We are also
grateful to all of the original observers and observatory staff who took
the data. We thank Laurie Urban for locating the University of Hawaii
2.2 m data on 67P, and Samuel Duddy for providing the rotational phase
corrections based on the Lowry et al. (2012) model. We are grateful to
Mike A'Hearn, Olivier Hainaut and Stephen Lowry for helpful suggestions.
The research leading to these results has received funding from the
European Union Seventh Framework Programme (FP7/2007-2013) under grant
agreement no. 268421. CS also thanks ESO's visiting scientist programme
for financial support during a visit to Garching, during which some of
this work was carried out. This research was supported in part by NASA
grants NNX13A151G and NNA09DA77A. We have used the NASA ADS system,
including the Dexter graph reading software, and thank the developers
and maintainers for their efforts. This research used the facilities of
the Canadian Astronomy Data Centre operated by the National Research
Council of Canada with the support of the Canadian Space Agency. Based
in part on data collected at Kiso observatory (University of Tokyo) and
obtained from the SMOKA, which is operated by the Astronomy Data Center,
National Astronomical Observatory of Japan. This research was made
possible through the use of the AAVSO Photometric All-Sky Survey
(APASS), funded by the Robert Martin Ayers Sciences Fund. We made use of
an image obtained by the SDSS, and calibrated other data based on their
star catalogue. Funding for SDSS-III has been provided by the Alfred P.
Sloan Foundation, the Participating Institutions, the National Science
Foundation, and the US 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,
University of Cambridge, 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.
NR 59
TC 34
Z9 34
U1 0
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 SEP
PY 2013
VL 557
AR A33
DI 10.1051/0004-6361/201322020
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 228TC
UT WOS:000325211900142
ER
PT J
AU Vornanen, T
Berdyugina, SV
Berdyugin, A
AF Vornanen, T.
Berdyugina, S. V.
Berdyugin, A.
TI Spectropolarimetric observations of cool DQ white dwarfs
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE molecular processes; white dwarfs; magnetic fields
ID DIGITAL SKY SURVEY; MODEL
AB Aims. Following our recent discovery of a new magnetic DQ white dwarf (WD) with CH molecular features, we report the results for the rest of the DQ WDs from our survey.
Methods. We use high signal-to-noise spectropolarimetric data to search for magnetic fields in a sample of 11 objects.
Results. One object in our sample, WD1235+422, shows the signs of continuum circular polarization that is similar to some peculiar DQs with unidentified molecular absorption bands, but the low signal-to-noise ratio and spectral resolution of these data make more observations necessary to reveal the true nature of this object.
C1 [Vornanen, T.] Univ Turku, Dept Phys & Astron, Piikkio 21500, Finland.
[Berdyugina, S. V.] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany.
[Berdyugina, S. V.] Univ Hawaii, Inst Astron, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
[Berdyugin, A.] Univ Turku, Finnish Ctr Astron ESO, Piikkio 21500, Finland.
RP Vornanen, T (reprint author), Univ Turku, Dept Phys & Astron, Vaisalantie 20, Piikkio 21500, Finland.
EM tommi.vornanen@utu.fi
FU Leibniz Association [SAW-2011-KIS-7]
FX This work was supported by the Leibniz Association grant SAW-2011-KIS-7.
NR 20
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 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2013
VL 557
AR A38
DI 10.1051/0004-6361/201220619
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 228TC
UT WOS:000325211900020
ER
PT J
AU Chamis, CC
Abdi, F
Garg, M
Minnetyan, L
Baid, H
Huang, D
Housner, J
Talagani, F
AF Chamis, Christos C.
Abdi, Frank
Garg, Mohit
Minnetyan, Levon
Baid, Harsh
Huang, Dade
Housner, Jerry
Talagani, Farid
TI Micromechanics-based progressive failure analysis prediction for
WWFE-III composite coupon test cases
SO JOURNAL OF COMPOSITE MATERIALS
LA English
DT Article
DE GENOA; damage; failure criteria; WWFE-III; open hole; multi-axial;
micromechanics; micro crack density
AB As a part of a world-wide study, a commercial code (General Optimization Analyzer), based on multi-scale (micro-macro) progressive failure analysis (PFA), is used to provide theoretical predictions for damage development for a set of challenging 13 test cases proposed in the Third World-Wide Failure Exercise (WWFE-III). Multiple failure criteria were utilized aimed at tackling issues related to a wide range of damage modes, being addressed by the WWFE-III. The critical damage events/indexes predictions tracked translaminar and interlaminar composite failures, namely matrix cracking/crack density, damage initiation/propagation, delamination initiation/growth, and their interaction with fiber failure. The composite laminates analysed were both with and without a central hole and the predictions were made using constituent fiber properties and matrix properties based on materials data or identification from ply stress-strain curve inputs. Loadings included uniaxial tension or compression, biaxial, bending, thermal, and loading-unloading.
C1 [Chamis, Christos C.] NASA, Glen Res Ctr, Cleveland, OH 44135 USA.
[Abdi, Frank; Garg, Mohit; Baid, Harsh; Huang, Dade; Housner, Jerry] AlphaSTAR Corp, Long Beach, CA USA.
[Minnetyan, Levon] Clarkson Univ, Potsdam, NY USA.
[Talagani, Farid] TU Delft Univ, Delft, Netherlands.
RP Chamis, CC (reprint author), NASA, Glen Res Ctr, 21000 Brookpk Rd,MS 49-7, Cleveland, OH 44135 USA.
EM Christos.C.Chamis@nasa.gov
NR 11
TC 15
Z9 15
U1 6
U2 18
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 SEP
PY 2013
VL 47
IS 20-21
SI SI
BP 2695
EP 2712
DI 10.1177/0021998313499478
PG 18
WC Materials Science, Composites
SC Materials Science
GA 220MO
UT WOS:000324588700015
ER
PT J
AU Russell, PS
Grant, JA
Williams, KK
Carter, LM
Garry, WB
Daubar, IJ
AF Russell, Patrick S.
Grant, John A.
Williams, Kevin K.
Carter, Lynn M.
Garry, W. Brent
Daubar, Ingrid J.
TI Ground penetrating radar geologic field studies of the ejecta of
Barringer Meteorite Crater, Arizona, as a planetary analog
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Impact ejecta; GPR; Meteor Crater; Size-frequency distribution; Mars;
Moon
ID SIZE-FREQUENCY DISTRIBUTIONS; MARS EXPLORATION; ELECTROMAGNETIC
PROPAGATION; MARTIAN SUBSURFACE; BRITTLE SOLIDS; FRAGMENT SIZE; LAVA
FLOWS; GPR; SCATTERING; FRACTURE
AB Ground penetrating radar (GPR) has been a useful geophysical tool in investigating a variety of shallow subsurface geological environments on Earth. Here we investigate the capabilities of GPR to provide useful geologic information in one of the most common geologic settings of planetary surfaces, impact crater ejecta. Three types of ejecta are surveyed with GPR at two wavelengths (400MHz, 200MHz) at Meteor Crater, Arizona, with the goal of capturing the GPR signature of the subsurface rock population. In order to ground truth the GPR characterization, subsurface rocks are visually counted and measured in preexisting subsurface exposures immediately adjacent to and below the GPR transect. The rock size-frequency distribution from 10 to 50cm based on visual counts is well described by both power law and exponential functions, the former slightly better, reflecting the control of fragmentation processes during the impact-ejection event. GPR counts are found to overestimate the number of subsurface rocks in the upper meter (by a factor of 2-3x) and underestimate in the second meter of depth (0.6-1.0x), results attributable to the highly scattering nature of blocky ejecta. Overturned ejecta that is fractured yet in which fragments are minimally displaced from their complement fragments produces fewer GPR returns than well-mixed ejecta. The use of two wavelengths and division of results into multiple depth zones provides multiple aspects by which to characterize the ejecta block population. Remote GPR measurement of subsurface ejecta in future planetary situations with no subsurface exposure can be used to characterize those rock populations relative to that of Meteor Crater.
C1 [Russell, Patrick S.; Grant, John A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
[Williams, Kevin K.] SUNY Buffalo State, Dept Earth Sci & Sci Educ, Buffalo, NY USA.
[Carter, Lynn M.; Garry, W. Brent] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Daubar, Ingrid J.] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Russell, PS (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315,POB 37012, Washington, DC 20013 USA.
EM russellp@si.edu
RI Carter, Lynn/D-2937-2012; Garry, Brent/I-5920-2013
FU NASA Lunar Science Institute [NNA09DB31A]
FX Many thanks to D. Kring, B. Andes, and the Barringer family for access
and guidance in performing research in the unique environment of Meteor
Crater. Appreciation is given for the time taken by Gwen Bart and an
anonymous reviewer for their helpful comments on the manuscript. This
research was carried out as part of the NASA Lunar Science Institute
team led by D. B. J. Bussey, Award #NNA09DB31A.
NR 79
TC 1
Z9 1
U1 0
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 SEP
PY 2013
VL 118
IS 9
BP 1915
EP 1933
DI 10.1002/jgre.20145
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 234FT
UT WOS:000325628300013
ER
PT J
AU Poppe, AR
Halekas, JS
Sarantos, M
Delory, GT
AF Poppe, A. R.
Halekas, J. S.
Sarantos, M.
Delory, G. T.
TI The self-sputtered contribution to the lunar exosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE lunar exosphere; pickup ions; self-sputtering
ID STEADY MAGNETOSPHERIC CONVECTION; PHOTON-STIMULATED DESORPTION; SHEET
BOUNDARY-LAYER; PLASMA SHEET; EARTHS MAGNETOTAIL; SODIUM EXOSPHERE;
ATMOSPHERE; ION; SURFACE; MOON
AB The lunar exosphere is produced by a combination of processes including thermal desorption, micrometeoroid bombardment, internal gas release, photon-stimulated desorption, and charged-particle sputtering. Here we investigate an additional mechanism not previously considered for the Moon, namely the role that newly born ions from the exosphere itself play in sputtering additional neutrals from the lunar surface, known as self-sputtering. Our calculations suggest that this process may sputter neutrals into the lunar exosphere at a rate equal to or greater than charged-particle sputtering due to passage through the Earth's plasma sheet when spatially averaged over the lunar dayside, while locally, self-sputtering may equal or exceed solar wind charged-particle sputtering and micrometeoroid bombardment. We use known or modeled densities and distributions of exospheric neutrals, laboratory-derived values for the photoionization rates and neutral sputtering yields, and knowledge of the ambient electromagnetic environment at the Moon to derive estimates of the self-sputtered neutral flux. We present the spatial variation of the self-sputtered neutral flux and discuss the implications thereof.
C1 [Poppe, A. R.; Halekas, J. S.; Delory, G. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Poppe, A. R.; Halekas, J. S.; Sarantos, M.; Delory, G. T.] NASA, Lunar Sci Inst, Ames Res Ctr, Mountain View, CA USA.
[Sarantos, M.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Sarantos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Poppe, AR (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM poppe@ssl.berkeley.edu
OI Poppe, Andrew/0000-0001-8137-8176; Halekas, Jasper/0000-0001-5258-6128
FU NASA Lunar Science Institute; NASA's Lunar Advanced Science and
Exploration Research program [NNX13AJ97G, NNX11AQ65G]
FX The authors gratefully acknowledge support from the NASA Lunar Science
Institute and NASA's Lunar Advanced Science and Exploration Research
program, grants NNX13AJ97G (A. R. P. and J.S.H.) and NNX11AQ65G (M. S.).
The authors are grateful to J. Cook and S. A. Stern at the Southwest
Research Institute for assistance in the interpretation of LRO/LAMP
exospheric results. A. R. P. and J. S. H. also acknowledge the
International Space Science Institute for hosting a workshop from which
this work benefitted.
NR 69
TC 3
Z9 3
U1 1
U2 8
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 SEP
PY 2013
VL 118
IS 9
BP 1934
EP 1944
DI 10.1002/jgre.20148
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 234FT
UT WOS:000325628300014
ER
PT J
AU Birn, J
Nakamura, R
Hesse, M
AF Birn, J.
Nakamura, R.
Hesse, M.
TI On the propagation of blobs in the magnetotail: MHD simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE blobs; entropy enhancement; magnetotail dynamics
ID BURSTY BULK FLOWS; CENTRAL PLASMA SHEET; AURORAL STREAMERS; MAGNETIC
RECONNECTION; THERMAL CATASTROPHE; FLUX TUBES; SUBSTORMS; TAIL;
INTENSIFICATIONS; INSTABILITY
AB Using three-dimensional magnetohydrodynamic (MHD) simulations of the magnetotail, we investigate the fate of entropy-enhanced localized magnetic flux tubes (blobs). Such flux tubes may be the result of a slippage process that also generates entropy-depleted flux tubes (bubbles) or of a rapid localized energy increase, for instance, from wave absorption. We confirm the expectation that the entropy enhancement leads to a tailward motion and that the speed and distance traveled into the tail increase with the entropy enhancement, even though the blobs tend to break up into pieces. The vorticity on the outside of the blobs twists the magnetic field and generates field-aligned currents predominantly of region-2 sense (earthward on the dusk side and tailward on the dawn side), which might provide a possibility for remote identification from the ground. The breakup, however, leads to more turbulent flow patterns, associated with opposite vorticity and the generation of region-1 sense field-aligned currents of lower intensity but approximately equal integrated magnitude.
C1 [Birn, J.] Space Sci Inst, Boulder, CO 80301 USA.
[Birn, J.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Nakamura, R.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
[Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Birn, J (reprint author), Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
EM jbirn@lanl.gov
RI Nakamura, Rumi/I-7712-2013; feggans, john/F-5370-2012; NASA MMS, Science
Team/J-5393-2013
OI Nakamura, Rumi/0000-0002-2620-9211; NASA MMS, Science
Team/0000-0002-9504-5214
FU US Department of Energy Los Alamos; NSF at Los Alamos; NASA at Los
Alamos
FX This work was performed mainly at Los Alamos under the auspices of the
US Department of Energy, supported by NSF's GEM and NASA's MMS/SMART
Theory and Modeling and SR&T Programs. We thank both referees for
stimulating "minor" comments and questions.
NR 39
TC 4
Z9 4
U1 0
U2 10
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 SEP
PY 2013
VL 118
IS 9
BP 5497
EP 5505
DI 10.1002/jgra.50521
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 232HN
UT WOS:000325483800010
ER
PT J
AU Hajra, R
Echer, E
Tsurutani, BT
Gonzalez, WD
AF Hajra, R.
Echer, E.
Tsurutani, B. T.
Gonzalez, W. D.
TI Solar cycle dependence of High-Intensity Long-Duration Continuous AE
Activity (HILDCAA) events, relativistic electron predictors?
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE HILDCAA; Auroral activity; Magnetosphere
ID COROTATING INTERACTION REGIONS; CORONAL MASS EJECTIONS; DST
LESS-THAN-OR-EQUAL-TO-50 NT; INTERPLANETARY MAGNETIC-FIELD; OUTER
RADIATION BELT; GEOMAGNETIC STORMS; WIND STREAMS; ALFVEN WAVES;
MAGNETOSPHERE; CHORUS
AB High-Intensity, Long-Duration, Continuous AE Activity (HILDCAA) events are studied using long-term geomagnetic and solar wind/interplanetary databases. We use the strict definition of a HILDCAA event, that it occurs outside of the main phase of a magnetic storm, the peak AE is >1000 nT, and the duration is at least 2 days long. One hundred thirty-three events have been identified from the AE indices in the 1975 to 2011 interval, a similar to 31/2 solar cycle span. Of the 133 events, 99 had simultaneous interplanetary data available. The overwhelmed majority (94%) of these latter cases were associated with high-speed solar wind stream (HSS) events. The remaining 6% of the cases occurred after the passage of interplanetary coronal mass ejections (ICMEs). The HSS-related events were typically associated with large interplanetary magnetic field (IMF) Bz variances. The ICME-related events were characterized by steady southward Bz intervals or low-frequency fluctuations, both of which we view as possible different interplanetary phenomena. HILDCAA events have been found to have their largest occurrence frequency in the solar cycle descending phase (similar to 6.8/year) with the second largest at solar minimum (similar to 3.5/year). The occurrence frequencies were considerably lower in the ascending phase (similar to 2.5/year) and at solar maximum (similar to 2.2/year). Thus, HILDCAAs can occur during all phases of the solar cycle, with the descending phase approximately three times more likely to have an event than at solar maximum and the ascending phase. The HILDCAA events that occurred in the declining phase and at solar minimum were >20% longer in duration than those in the ascending phase and solar maximum, respectively. The events during the recent solar and geomagnetic minima, 2007-2009, were, on the average, similar to 17% and 14% weaker in peak AE than the events during the previous two minima of 1995-1997 and 1985-1987, respectively. The recent minimum events were similar to 35% and 41% shorter in durations, respectively, than the events during those previous minima. The yearly occurrence of the events exhibited statistically significant correlation (>0.70) with yearly average speed and number of HSSs. No seasonal dependence of HILDCAA was noted.
C1 [Hajra, R.; Echer, E.; Gonzalez, W. D.] Inst Nacl Pesquisas Espaciais, Sao Paulo, Brazil.
[Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Hajra, R (reprint author), Inst Nacl Pesquisas Espaciais, Av Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
EM rajkumarhajra@yahoo.co.in
RI Hajra, Rajkumar/C-1246-2011;
OI Hajra, Rajkumar/0000-0003-1583-182X; Hajra, Rajkumar/0000-0003-0447-1531
FU FundacAo de Amparo a Pesquisa do Estado de SAo Paulo (FAPESP) through
post-doctoral research fellowship at INPE; Brazilian CNPq agency
[301233/2011-0]
FX The work of RH is financially supported by FundacAo de Amparo a Pesquisa
do Estado de SAo Paulo (FAPESP) through post-doctoral research
fellowship at INPE. One of the authors (EE) would like to thank the
Brazilian CNPq (301233/2011-0) agency for financial support. Portions of
this research were performed at the Jet Propulsion Laboratory,
California Institute of Technology under contract with NASA. BTT wishes
to thank P. Bellan for hosting him at the Applied Physics Department
during his sabbatical stay at Caltech and M. Paetzold during his stay at
the University of Cologne, Germany.
NR 82
TC 18
Z9 18
U1 1
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 SEP
PY 2013
VL 118
IS 9
BP 5626
EP 5638
DI 10.1002/jgra.50530
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 232HN
UT WOS:000325483800021
ER
PT J
AU Meng, X
Toth, G
Glocer, A
Fok, MC
Gombosi, TI
AF Meng, X.
Toth, G.
Glocer, A.
Fok, M-C
Gombosi, T. I.
TI Pressure anisotropy in global magnetospheric simulations: Coupling with
ring current models
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE pressure anisotropy; MHD modeling; ring current
ID PLASMA PRESSURE; MAGNETIC-FIELD; MAGNETOHYDRODYNAMICS; DISTRIBUTIONS;
REGION; SHEET; CODE; LFM
AB We have recently extended the global magnetohydrodynamic (MHD) model BATS-R-US to account for pressure anisotropy. Since the inner magnetosphere dynamics cannot be fully described even by anisotropic MHD, we coupled our anisotropic MHD model with two inner magnetospheric models: the Rice Convection Model (RCM) and the Comprehensive Ring Current Model (CRCM). The coupled models provide better representations of the near-Earth plasma, especially during geomagnetic storms. In this paper, we present the two-way coupling algorithms with both ring current models. The major difference between these two couplings is that the RCM assumes isotropic and constant pressures along closed field lines, while the CRCM resolves pitch angle anisotropy. For model validation, we report global magnetosphere simulations performed by the coupled models. The simulation results are compared to the results given by the coupled isotropic MHD and ring current models. We find that in the global MHD simulations coupled with ring current models, pressure anisotropy results in a thinner magnetosheath, a shorter tail, a much smaller Earthward plasma jet from the tail reconnection site, and is also important in controlling the magnetic field configuration. The comparisons with satellite data for the magnetospheric event simulations show improvements on reproducing the measured tail magnetic field and inner magnetospheric flow velocity when including pressure anisotropy in the ring current model coupled global MHD model.
C1 [Meng, X.; Toth, G.; Gombosi, T. I.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Glocer, A.; Fok, M-C] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Meng, X (reprint author), Univ Michigan, Ctr Space Environm Modeling, 2455 Hayward St, Ann Arbor, MI 48109 USA.
EM xingm@umich.edu
RI Toth, Gabor/B-7977-2013; feggans, john/F-5370-2012; Glocer,
Alex/C-9512-2012; Fok, Mei-Ching/D-1626-2012; Meng, Xing/A-1929-2016;
Gombosi, Tamas/G-4238-2011
OI Toth, Gabor/0000-0002-5654-9823; Glocer, Alex/0000-0001-9843-9094;
Gombosi, Tamas/0000-0001-9360-4951
FU NASA; NSF
FX The authors thank Andrei Runov and the THEMIS team for providing the
THEMIS data. The authors also acknowledge N. Ness at Bartol Research
Institute, D. J. McComas at SWRI, K. Ogilvie at NASA GSFC and CDAweb for
providing the IMF and solar wind data from ACE and WIND, S. Kakugun at
STELAB Nagoya Univ., and CDAweb for providing the Geotail data, and H.
Singer at NOAA SEC and CDAweb for providing the GOES data. The SYM-H
data is taken from the World Data Center (WDC) for Geomagnetism, Kyoto.
This work was supported by various research grants from NASA and NSF.
The computing resources were provided by the NASA High-End Computing
(HEC) Program through the NASA Advanced Supercomputing (NAS) Division at
Ames Research Center.
NR 35
TC 7
Z9 7
U1 0
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 SEP
PY 2013
VL 118
IS 9
BP 5639
EP 5658
DI 10.1002/jgra.50539
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 232HN
UT WOS:000325483800022
ER
PT J
AU Katz, I
AF Katz, I.
TI Comment on "Electromagnetic pulses generated by meteoroid impacts on
spacecraft" by S. Close, P. Colestock, L. Cox, M. Kelley, and N. Lee
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Editorial Material
DE meteoroid impact
ID PLASMA; EXPANSION; VACUUM
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Katz, I (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ikatz@jpl.nasa.gov
NR 9
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 SEP
PY 2013
VL 118
IS 9
BP 5803
EP 5805
DI 10.1002/jgra.50536
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 232HN
UT WOS:000325483800035
ER
PT J
AU Sonnabend, G
Stupar, D
Sornig, M
Stangier, T
Kostiuk, T
Livengood, TA
AF Sonnabend, G.
Stupar, D.
Sornig, M.
Stangier, T.
Kostiuk, T.
Livengood, T. A.
TI A search for methane in the atmosphere of Mars using ground-based mid
infrared heterodyne spectroscopy
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Planetary atmosphere; Remote sensing; Spectroscopy; Methane
ID WIND; CO2
AB We report our search for methane in the atmosphere of Mars using high-spectral resolution heterodyne spectroscopy in the 7.8 mu m wavelength region. Resolving power and frequency precision of >10(6) of the technique enable identification and full resolution of a targeted spectral line in the terrestrial-Mars spectrum observed from the ground. Observations were carried out on two occasions, in April 2010 and May 2012 at the McMath-Pierce Solar Telescope and the NASA Infrared Telescope Facility, respectively. A single line in the nu 4 band of methane at 1282.62448 cm(-1) was targeted in both cases. No absorption due to methane was detected and only upper limits of 100 ppb for the martian atmospheric methane concentration were retrieved. Lack of observing time (due to weather) and telluric opacity greater than anticipated led to reduced signal-to-noise ratios (SNR). Based on current measurements and calculations, under proper viewing conditions, we estimate an achievable detection limit of similar to 10 ppb using the infrared heterodyne technique - adequate for confirming reported detections of methane based on other techniques. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Sonnabend, G.; Stupar, D.; Stangier, T.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
[Sornig, M.] Univ Cologne, Rhein Inst Umweltforsch, Abt Planetenforsch, D-50931 Cologne, Germany.
[Kostiuk, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Livengood, T. A.] NASA, CRESST, UMD, GSFC, Greenbelt, MD 20771 USA.
RP Sonnabend, G (reprint author), Univ Cologne, Inst Phys 1, Zuelpicher Str 77, D-50937 Cologne, Germany.
EM samstag@ph1.uni-koeln.de
RI Kostiuk, Theodor/A-3077-2014
FU Deutsche Forschungsgemeinschaft (DFG) [SO879/3-1, SO879/4-1]
FX The authors thank the directors and staff of the NASA Infrared Telescope
Facility and the McMath Solar Observatory for their support of infrared
heterodyne observations. We also thank our reviewers for many helpful
comments. This work was supported by the Deutsche Forschungsgemeinschaft
(DFG) through Grants SO879/3-1 and SO879/4-1.
NR 21
TC 1
Z9 1
U1 1
U2 11
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD SEP
PY 2013
VL 291
SI SI
BP 98
EP 101
DI 10.1016/j.jms.2013.05.009
PG 4
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 234TA
UT WOS:000325666000013
ER
PT J
AU Gustin, J
Gerard, JC
Grodent, D
Gladstone, GR
Clarke, JT
Pryor, WR
Dols, V
Bonfond, B
Radioti, A
Lamy, L
Ajello, JM
AF Gustin, J.
Gerard, J-C
Grodent, D.
Gladstone, G. R.
Clarke, J. T.
Pryor, W. R.
Dols, V.
Bonfond, B.
Radioti, A.
Lamy, L.
Ajello, J. M.
TI Effects of methane on giant planet's UV emissions and implications for
the auroral characteristics
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Ultraviolet; Giant planets; H2 spectroscopy; Methane; Aurora; Atmosphere
ID EXTREME-ULTRAVIOLET OBSERVATIONS; DISSOCIATION CROSS-SECTIONS; JOVIAN
AURORA; SPECTROMETER OBSERVATIONS; ELECTRON-PRECIPITATION; SPECTRAL
OBSERVATIONS; VOYAGER-1 ENCOUNTER; THERMAL STRUCTURE; PHOTOABSORPTION;
ABSORPTION
AB This study reviews methods used to determine important characteristics of giant planet's UV aurora (brightness, energy of the precipitating particles, altitude of the emission peak, ...), based on the absorbing properties of methane and other hydrocarbons. Ultraviolet aurorae on giant planets are mostly caused by inelastic collisions between energetic magnetospheric electrons and the ambient atmospheric H-2 molecules. The auroral emission is situated close to a hydrocarbon layer and may be attenuated by methane (CH4), ethane (C2H6) and acetylene (C2H2) at selected wavelengths. As methane is the most abundant hydrocarbon, it is the main UV absorber and attenuates the auroral emission shorward of 1350 angstrom. The level of absorption is used to situate the altitude/pressure level of the aurora, hence the energy of the precipitated electrons, whose penetration depth is directly related to their mean energy. Several techniques are used to determine these characteristics, from the color ratio method which measures the level of absorption from the ratio between an absorbed and an unabsorbed portion of the observed auroral spectrum, to more realistic methods which combine theoretical distributions of the precipitating electrons with altitude dependent atmospheric models. The latter models are coupled with synthetic or laboratory H-2 spectra and the simulated emergent spectra are compared to observations to determine the best auroral characteristics.
Although auroral characteristics may be very variable with time and locations, several typical properties may be highlighted from these methods: the Jovian aurora is the most powerful, with brightness around 120 kR produced by electrons of mean energy similar to 100 key and an emission situated near the 1 gbar level (similar to 250 km above the 1 bar level) while Saturn's aurora is fainter (similar to 10 kR), produced by electrons less than 20 keV and situated near the 0.2 mu bar level (similar to 1100 km). (C) 2013 Elsevier Inc. All rights reserved.
C1 [Gustin, J.; Gerard, J-C; Grodent, D.; Bonfond, B.; Radioti, A.] Univ Liege, Lab Phys Atmospher & Planetaire, Liege, Belgium.
[Gladstone, G. R.] SW Res Inst, San Antonio, TX USA.
[Clarke, J. T.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA.
[Pryor, W. R.] Cent Arizona Coll, Coolidge, AZ USA.
[Dols, V.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Lamy, L.] Univ Paris Diderot, Observ Paris, Lab Etud Spatiales & Instrumentat Astrophys, Meudon, France.
[Ajello, J. M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Gustin, J (reprint author), Univ Liege, Lab Phys Atmospher & Planetaire, Liege, Belgium.
EM gustin@astro.ulg.ac.be
RI Clarke, John/C-8644-2013;
OI Bonfond, Bertrand/0000-0002-2514-0187; GERARD,
Jean-Claude/0000-0002-8565-8746
FU NASA; Cassini Project; Belgian Fund for Scientific Research (FNRS);
PRODEX program of ESA; University of Liege
FX Financial support to US participants was provided by NASA and the
Cassini Project. J.-C.G. and A.R. acknowledge support from the Belgian
Fund for Scientific Research (FNRS). The PRODEX program of ESA and the
University of Liege provided financial support for this research.
NR 59
TC 11
Z9 11
U1 2
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD SEP
PY 2013
VL 291
SI SI
BP 108
EP 117
DI 10.1016/j.jms.2013.03.010
PG 10
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 234TA
UT WOS:000325666000015
ER
PT J
AU Gibb, EL
Bonev, BP
Villanueva, G
DiSanti, MA
Mumma, MJ
AF Gibb, Erika L.
Bonev, Boncho P.
Villanueva, Geronimo
DiSanti, Michael A.
Mumma, Michael J.
TI Solar fluorescence model of CH3D as applied to comet emission
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Methane; Fluorescence; Comets; Model
ID YOUNG CIRCUMSTELLAR DISKS; C/2004 Q2 MACHHOLZ; ORGANIC-MOLECULES; SPIN
TEMPERATURE; WATER; METHANE; CM(-1); SPECTRUM; RATIO; II.
AB We developed a solar fluorescence emission model for the v(4) band of CH3D for application to low-density, optically thin environments like cometary atmospheres. Our model utilizes transition frequencies, energy levels, and line strengths from the HITRAN 2008 database. We calculated the statistical weights of states with A-type and E-type spin symmetry, the partition functions for each spin manifold as a function of rotational temperature, and the Einstein A- and B-coefficients for individual rotational-vibrational transitions. We used these parameters to construct a database of fluorescence efficiencies (g-factors) at rotational temperatures relevant to cometary atmospheres. The effects of nuclear spin temperature and rotational temperature on the resulting g-factors are disentangled and modeled separately. The primary application of this model is to constrain the abundance ratio CH3D/CH4 in cometary ice, a possible cosmogonic parameter. We present the upper limit for CH3D/CH4 in comet C/2007 N3 (Lulin) using our model and illustrate the ability of current spectrometers to stringently constrain astrochemical model predictions for CH3D/CH4 in the early solar system. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Gibb, Erika L.] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA.
[Bonev, Boncho P.; Villanueva, Geronimo] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Bonev, Boncho P.; Villanueva, Geronimo; DiSanti, Michael A.; Mumma, Michael J.] NASA, Goddard Ctr Astrobiol, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gibb, EL (reprint author), Univ Missouri, Dept Phys & Astron, 503 Benton Hall,1 Univ Blvd, St Louis, MO 63121 USA.
EM gibbe@umsl.edu
FU NSF Planetary Astronomy grants [AST-0807939, AST-1211362]; NASA's
Planetary Atmospheres and Astronomy Programs [08-PATM08-0031,
09-PATM09-0080, 08-PAST08-0033/34, 09-PAST09-0034]; NASA's Astrobiology
Institute [NAI5/NNH08ZDA002C]; W.M. Keck Foundation
FX BPB and ELG were supported by NSF Planetary Astronomy grants AST-0807939
and AST-1211362. GLV, MAD and MJM acknowledge support from NASA's
Planetary Atmospheres and Astronomy Programs (08-PATM08-0031 (PI: GLV),
09-PATM09-0080 (PI: MAD), 08-PAST08-0033/34 (PI: MJM), 09-PAST09-0034
(PI: MAD)), and NASA's Astrobiology Institute (NAI5/NNH08ZDA002C, PI:
MJM).; The spectra presented herein 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
the National Aeronautics and Space Administration. The Observatory was
made possible by the generous financial support of the W.M. Keck
Foundation. The authors recognize and acknowledge the very significant
cultural role and reverence that the summit of Mauna Kea has always had
within the indigenous Hawaiian community.
NR 38
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 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD SEP
PY 2013
VL 291
SI SI
BP 118
EP 124
DI 10.1016/j.jms.2013.05.007
PG 7
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 234TA
UT WOS:000325666000016
ER
PT J
AU Mader, TH
Gibson, CR
Pass, AF
Lee, AG
Killer, HE
Hansen, HC
Dervay, JP
Barratt, MR
Tarver, WJ
Sargsyan, AE
Kramer, LA
Riascos, R
Bedi, DG
Pettit, DR
AF Mader, Thomas H.
Gibson, C. Robert
Pass, Anastas F.
Lee, Andrew G.
Killer, Hanspeter E.
Hansen, Hans-Christian
Dervay, Joseph P.
Barratt, Michael R.
Tarver, William J.
Sargsyan, Ashot E.
Kramer, Larry A.
Riascos, Roy
Bedi, Deepak G.
Pettit, Donald R.
TI Optic Disc Edema in an Astronaut After Repeat Long-Duration Space Flight
SO JOURNAL OF NEURO-OPHTHALMOLOGY
LA English
DT Article
ID PRESSURE; NERVE
AB Background:A number of ophthalmic findings including optic disc edema, globe flattening, and choroidal folds have been observed in several astronauts after long-duration space flights. The authors report the first astronaut with previously documented postflight ophthalmic abnormalities who developed new pathological changes after a repeat long-duration mission.Methods:A case study of an astronaut with 2 long-duration (6 months) exposures to microgravity. Before and after his first long-duration space flight, he underwent complete eye examination, including fundus photography. Before and after his second flight, 9 years later, he underwent fundus photography, optical coherence tomography, ocular ultrasonography, and brain magnetic resonance imaging, as well as in-flight fundus photography and ultrasound.Results:After his first long-duration mission, the astronaut was documented to have eye findings limited to unilateral choroidal folds and a single cotton wool spot. During a subsequent 6-month mission, he developed more widespread choroidal folds and new onset of optic disc edema in the same eye.Conclusion:Microgravity-induced anatomical changes that occurred during the first mission may have set the stage for recurrent or additional changes when the astronaut was subjected to physiological stress of repeat space flight.
C1 [Mader, Thomas H.] Alaska Native Med Ctr, Dept Ophthalmol, Anchorage, AK USA.
[Gibson, C. Robert] Coastal Eye Associates, Webster, TX USA.
[Pass, Anastas F.] Univ Houston, Univ Eye Inst, Houston, TX USA.
[Lee, Andrew G.] Methodist Hosp, Dept Ophthalmol, Houston, TX 77030 USA.
[Killer, Hanspeter E.] Kantonsspital Aarau, Dept Ophthalmol, Aarau, Switzerland.
[Hansen, Hans-Christian] Univ Hosp Hamburg Eppendorf, Dept Neurol & Psychiat, Hamburg, Germany.
[Dervay, Joseph P.; Barratt, Michael R.; Tarver, William J.; Pettit, Donald R.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Sargsyan, Ashot E.] Wyle Sci Technol & Engn, Houston, TX USA.
[Kramer, Larry A.] Univ Texas Hlth Sci Ctr Houston, Dept Diagnost Imaging & Intervent, Houston, TX 77030 USA.
[Riascos, Roy] Univ Texas Med Branch Galveston, Galveston, TX USA.
[Bedi, Deepak G.] Univ Texas MD Anderson Canc Ctr, Houston, TX 77030 USA.
RP Mader, TH (reprint author), 6550 Farpoint Dr, Anchorage, AK 99507 USA.
EM tmader@acsalaska.net
OI Riascos, Roy/0000-0002-3081-0413
NR 19
TC 16
Z9 16
U1 0
U2 10
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 1070-8022
EI 1536-5166
J9 J NEURO-OPHTHALMOL
JI J. Neuro-Ophthal.
PD SEP
PY 2013
VL 33
IS 3
BP 249
EP 255
DI 10.1097/WNO.0b013e31829b41a6
PG 7
WC Clinical Neurology; Ophthalmology
SC Neurosciences & Neurology; Ophthalmology
GA 235GC
UT WOS:000325704000012
PM 23851997
ER
PT J
AU Mazuruk, K
Volz, MP
AF Mazuruk, K.
Volz, M. P.
TI Static stability of menisci in detached Bridgman growth
SO PHYSICS OF FLUIDS
LA English
DT Article
ID CAPILLARY SURFACES; ZERO-GRAVITY; DYNAMICS; SOLIDS; ZONE
AB A static stability analysis is performed for the menisci that form above the crystal-crucible gap during detached Bridgman growth. The sign of the second variation of the potential energy against admissible meniscus shape perturbations is considered as the stability criterion. Parameters governing the stability are the pressure differential across the meniscus, the Bond number, the crystal radius, the growth angle between the crystal and melt, and the contact angle between the melt and the crucible. The effects on stability of confined gases adjacent to the meniscus are also examined. Axisymmetric as well as non-axisymmetric perturbations are investigated. Axisymmetric perturbation modes require coupling to the meniscus that exists at the top of the melt to ensure melt volume preservation. Both rough and microscopically smooth interior crucible surfaces, corresponding to pinned and unpinned states, are considered. Pinning extends the parameter range over which menisci are stable. The symmetry of the least stable perturbation mode depends on the Bond number and whether the menisci are pinned. For Bond numbers equal to zero, corresponding to zero gravity conditions, all menisci are statically stable. (C) 2013 AIP Publishing LLC.
C1 [Mazuruk, K.] Univ Alabama, Huntsville, AL 35899 USA.
[Volz, M. P.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Volz, MP (reprint author), NASA, George C Marshall Space Flight Ctr, EM31, Huntsville, AL 35812 USA.
EM Martin.Volz@nasa.gov
FU U.S. National Aeronautics and Space Administration [NNM11AA01A]
FX This research was supported by the U.S. National Aeronautics and Space
Administration under cooperative agreement NNM11AA01A.
NR 26
TC 2
Z9 2
U1 0
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-6631
EI 1089-7666
J9 PHYS FLUIDS
JI Phys. Fluids
PD SEP
PY 2013
VL 25
IS 9
AR 094106
DI 10.1063/1.4821849
PG 13
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 231EU
UT WOS:000325397800053
ER
PT J
AU Aunai, N
Hesse, M
Kuznetsova, M
AF Aunai, Nicolas
Hesse, Michael
Kuznetsova, Maria
TI Electron nongyrotropy in the context of collisionless magnetic
reconnection
SO PHYSICS OF PLASMAS
LA English
DT Article
AB Collisionless magnetized plasmas have the tendency to isotropize their velocity distribution function around the local magnetic field direction, i.e., to be gyrotropic, unless some spatial and/or temporal fluctuations develop at the particle gyroscales. Electron gyroscale inhomogeneities are well known to develop during the magnetic reconnection process. Nongyrotropic electron velocity distribution functions have been observed to play a key role in the dissipative process breaking the field line connectivity. In this paper, we present a new method to quantify the deviation of a particle population from gyrotropy. The method accounts for the full 3D shape of the distribution and its analytical formulation allows fast numerical computation. Regions associated with a significant degree of nongyrotropy are shown, as well as the kinetic origin of the nongyrotropy and the fluid signature it is associated with. Using the result of 2.5D Particle-In-Cell simulations of magnetic reconnection in symmetric and asymmetric configurations, it is found that neither the reconnection site nor the topological boundaries are generally associated with a maximized degree of nongyrotropy. Nongyrotropic regions do not correspond to a specific fluid behavior as equivalent nongyrotropy is found to extend over the electron dissipation region as well as in non-dissipative diamagnetic drift layers. The localization of highly nongyrotropic regions in numerical models and their correlation with other observable quantities can, however, improve the characterization of spatial structures explored by spacecraft missions. (C) 2013 AIP Publishing LLC.
C1 [Aunai, Nicolas; Hesse, Michael; Kuznetsova, Maria] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Aunai, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM nicolas.aunai@nasa.gov
RI feggans, john/F-5370-2012; NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NASA
FX The authors kindly thank Deirdre Wendel for very useful discussions.
N.A. acknowledges support from the NASA postdoctoral program. M. H.
acknowledges support from the theory and modeling group of NASA's MMS.
NR 15
TC 26
Z9 26
U1 1
U2 4
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD SEP
PY 2013
VL 20
IS 9
AR 092903
DI 10.1063/1.4820953
PG 6
WC Physics, Fluids & Plasmas
SC Physics
GA 231FE
UT WOS:000325399400059
ER
PT J
AU Abraham, JP
Baringer, M
Bindoff, NL
Boyer, T
Cheng, LJ
Church, JA
Conroy, JL
Domingues, CM
Fasullo, JT
Gilson, J
Goni, G
Good, SA
Gorman, JM
Gouretski, V
Ishii, M
Johnson, GC
Kizu, S
Lyman, JM
Macdonald, AM
Minkowycz, WJ
Moffitt, SE
Palmer, MD
Piola, AR
Reseghetti, F
Schuckmann, K
Trenberth, KE
Velicogna, I
Willis, JK
AF Abraham, J. P.
Baringer, M.
Bindoff, N. L.
Boyer, T.
Cheng, L. J.
Church, J. A.
Conroy, J. L.
Domingues, C. M.
Fasullo, J. T.
Gilson, J.
Goni, G.
Good, S. A.
Gorman, J. M.
Gouretski, V.
Ishii, M.
Johnson, G. C.
Kizu, S.
Lyman, J. M.
Macdonald, A. M.
Minkowycz, W. J.
Moffitt, S. E.
Palmer, M. D.
Piola, A. R.
Reseghetti, F.
Schuckmann, K.
Trenberth, K. E.
Velicogna, I.
Willis, J. K.
TI A REVIEW OF GLOBAL OCEAN TEMPERATURE OBSERVATIONS: IMPLICATIONS FOR
OCEAN HEAT CONTENT ESTIMATES AND CLIMATE CHANGE
SO REVIEWS OF GEOPHYSICS
LA English
DT Review
DE global warming; ocean heat content; Argo float; thermosteric sea level
rise; expendable bathythermograph; Earth energy balance
ID SEA-LEVEL RISE; EXPENDABLE BATHYTHERMOGRAPH XBT; EARTHS ENERGY
IMBALANCE; WESTERN SOUTH-ATLANTIC; THETA-S CLIMATOLOGY; FALL-RATE;
PROFILING FLOATS; SUBSURFACE TEMPERATURE; SURFACE TEMPERATURES; CONTENT
VARIABILITY
AB The evolution of ocean temperature measurement systems is presented with a focus on the development and accuracy of two critical devices in use today (expendable bathythermographs and conductivity-temperature-depth instruments used on Argo floats). A detailed discussion of the accuracy of these devices and a projection of the future of ocean temperature measurements are provided. The accuracy of ocean temperature measurements is discussed in detail in the context of ocean heat content, Earth's energy imbalance, and thermosteric sea level rise. Up-to-date estimates are provided for these three important quantities. The total energy imbalance at the top of atmosphere is best assessed by taking an inventory of changes in energy storage. The main storage is in the ocean, the latest values of which are presented. Furthermore, despite differences in measurement methods and analysis techniques, multiple studies show that there has been a multidecadal increase in the heat content of both the upper and deep ocean regions, which reflects the impact of anthropogenic warming. With respect to sea level rise, mutually reinforcing information from tide gauges and radar altimetry shows that presently, sea level is rising at approximately 3mmyr(-1) with contributions from both thermal expansion and mass accumulation from ice melt. The latest data for thermal expansion sea level rise are included here and analyzed.
C1 [Abraham, J. P.; Gorman, J. M.] Univ St Thomas, Sch Engn, St Paul, MN 55105 USA.
[Baringer, M.; Goni, G.] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA.
[Bindoff, N. L.] Univ Tasmania, IMAS, Hobart, Tas, Australia.
[Bindoff, N. L.; Church, J. A.] CSIRO Marine & Atmospher Res, Ctr Australian Weather & Climate Res, Hobart, Tas, Australia.
[Bindoff, N. L.; Domingues, C. M.] Univ Tasmania, Antarctic Climate & Ecosyst Cooperat Res Ctr, Hobart, Tas, Australia.
[Boyer, T.] NOAA, Natl Oceanog Data Ctr, Silver Spring, MD USA.
[Cheng, L. J.] Chinese Acad Sci, Inst Atmospher Phys, Beijing, Peoples R China.
[Conroy, J. L.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Fasullo, J. T.; Trenberth, K. E.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Gilson, J.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Good, S. A.; Palmer, M. D.] Met Off Hadley Ctr, Exeter, Devon, England.
[Gouretski, V.] Univ Hamburg, Hamburg, Germany.
[Ishii, M.] Meteorol Res Inst, Climate Res Dept, Tsukuba, Ibaraki 305, Japan.
[Johnson, G. C.; Lyman, J. M.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA.
[Kizu, S.] Tohoku Univ, Dept Geophys, Sendai, Miyagi 980, Japan.
[Lyman, J. M.] Univ Hawaii Manoa, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA.
[Macdonald, A. M.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Minkowycz, W. J.] Univ Illinois, Dept Mech & Ind Engn, Chicago, IL USA.
[Moffitt, S. E.] Bodega Bay Marine Lab, Bodega Bay, CA USA.
[Moffitt, S. E.] Univ Calif Davis, Grad Grp Ecol, Davis, CA 95616 USA.
[Piola, A. R.] Univ Buenos Aires, Dept Oceanog, Serv Hidrografia Naval, Buenos Aires, DF, Argentina.
[Piola, A. R.] Univ Buenos Aires, UMI IFAECI, Dept Ciencias Atmosfera & Oceanos, Buenos Aires, DF, Argentina.
[Reseghetti, F.] ENEA Italian Natl Agcy New Technol, Energy Sustainable Econ Dev UTMAR OSS, La Spezia, Italy.
[Schuckmann, K.] IFREMER, Toulon, France.
[Velicogna, I.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Velicogna, I.; Willis, J. K.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Abraham, JP (reprint author), Univ St Thomas, Sch Engn, 2115 Summit Ave, St Paul, MN 55105 USA.
EM jpabraham@stthomas.edu
RI Bindoff, Nathaniel/C-8050-2011; Goni, Gustavo/D-2017-2012; Johnson,
Gregory/I-6559-2012; Church, John/A-1541-2012; Piola,
Alberto/O-2280-2013; Baringer, Molly/D-2277-2012; Domingues, Catia
/A-2901-2015; Trenberth, Kevin/A-5683-2012
OI Bindoff, Nathaniel/0000-0001-5662-9519; Goni,
Gustavo/0000-0001-7093-3170; Gorman, John/0000-0003-4046-7847; Johnson,
Gregory/0000-0002-8023-4020; Church, John/0000-0002-7037-8194; Piola,
Alberto/0000-0002-5003-8926; Baringer, Molly/0000-0002-8503-5194;
Domingues, Catia /0000-0001-5100-4595; Trenberth,
Kevin/0000-0002-1445-1000
FU ARC Centre of Excellence for Climate Systems Science; MOST project
[2012CB417404]; Australian Climate Change Science Program; Australian
Antarctic and Ecosystems Research Cooperative Centre; NOAA [NA17RJ1231];
DECC/Defra Met Office Hadley Centre Climate Programme [GA01101]; Cluster
of Excellence "CLISAP", University of Hamburg [EXC177]; German Science
Foundation; NOAA Climate Program Office; NOAA Research; Inter-American
Institute for Global Change Research through the US National Science
Foundation [GEO-0452325]; NASA [NNX09AH89G]; EC FP7 project MyOcean2
FX N.L.B. acknowledges support from the ARC Centre of Excellence for
Climate Systems Science. L.J.C. was supported by the MOST project (grant
2012CB417404). J.A.C. and S. W. were funded by the Australian Climate
Change Science Program. C. M. D. was funded by the Australian Antarctic
and Ecosystems Research Cooperative Centre. J.G. was supported through
NOAA grant NA17RJ1231 (Scripps Institute of Oceanography). S. A. G. was
supported by the Joint DECC/Defra Met Office Hadley Centre Climate
Programme (GA01101). V. G. was supported through the Cluster of
Excellence "CLISAP" (EXC177), University of Hamburg, funded through the
German Science Foundation. T. B., J.M.L., and G.C.J. were supported by
the NOAA Climate Program Office and NOAA Research. A. P. was supported
by the Inter-American Institute for Global Change Research through the
US National Science Foundation grant GEO-0452325. K. E. T. and J.T.F.
were sponsored by NASA under grant NNX09AH89G. F. R. was supported by EC
FP7 project MyOcean2 and operationally supported in part by NOAA/AOML.
NR 196
TC 76
Z9 79
U1 15
U2 162
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 8755-1209
EI 1944-9208
J9 REV GEOPHYS
JI Rev. Geophys.
PD SEP
PY 2013
VL 51
IS 3
BP 450
EP 483
DI 10.1002/rog.20022
PG 34
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 232LV
UT WOS:000325496200003
ER
PT J
AU Thedinga, JF
Johnson, SW
Neff, AD
Hoffman, CA
Maselko, JM
AF Thedinga, John F.
Johnson, Scott W.
Neff, A. Darcie
Hoffman, Chris A.
Maselko, Jacek M.
TI Nearshore Fish Assemblages of the Northeastern Chukchi Sea, Alaska
SO ARCTIC
LA English
DT Article
DE Arctic; Alaska; Chukchi Sea; nearshore; Arctic cod; capelin; beach
seine; bottom trawl
ID COD BOREOGADUS-SAIDA; CAPELIN MALLOTUS-VILLOSUS; BEAUFORT SEA; ARCTIC
COD; COASTAL WATERS; BARENTS SEA; COMMUNITY; DEMERSAL; PREDATION
AB The Arctic ecosystem is changing rapidly, yet information on nearshore fish assemblages for the northeastern Chukchi Sea is extremely limited. To address this information gap, we sampled nearshore fish assemblages with a beach seine and a small bottom trawl at six stations in the northeastern Chukchi Sea in August 2007, 2008, and 2009, and in September 2009. Catch and species composition differed by gear type and between sample periods, including the two in 2009. A total of 16 039 fish representing 18 species were captured in 24 beach seine hauls, and 3108 fish representing 24 species were captured in 48 trawl tows. Beach seine catch was dominated by capelin (83%), and trawl catch was dominated by Arctic cod (56%). Species that were good discriminators between gear types were capelin (seine) and slender eelblenny (trawl), and unidentified small sculpins were the most common taxa caught with both gear types. Capelin and Arctic cod captured by either gear type were mostly juveniles (judging by size). Variability among sampling periods in catch and species composition within gear types can likely be attributed to annual variations in environmental conditions, including differences in water temperature (range: 2 degrees-9 degrees C). The shallow nearshore environment of the northeastern Chukchi Sea provides important habitat for many fish species and is extremely vulnerable to disturbance. Loss of sea ice from global warming may open up formerly inaccessible areas to oil and gas exploration, vessel traffic, and commercial fishing. Thus, long-term monitoring of nearshore fish assemblages in the Alaskan Arctic is necessary for managers to make informed decisions in this fragile environment.
C1 [Thedinga, John F.; Johnson, Scott W.; Neff, A. Darcie; Maselko, Jacek M.] Natl Ocean & Atmospher Adm, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Juneau, AK 99801 USA.
[Hoffman, Chris A.] US Army Corps Engineers, Elmendorf AFB, AK 99506 USA.
RP Thedinga, JF (reprint author), Natl Ocean & Atmospher Adm, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM jthedinga@gci.net
FU NOAA's Essential Fish Habitat Program at the Auke Bay Laboratories of
the Alaska Fisheries Science Center
FX We especially thank Craig George and the North Slope Borough for
providing the invaluable field and logistical support that made this
study possible. We also thank Andres Lopez, Estrella Campellone, Dugan
Greenwell, John Eiler, Kim Fackler, Mark Carls, and Valerie Palmer for
help in the field. We thank Adam Moles for reviewing this manuscript.
This project was partially funded by NOAA's Essential Fish Habitat
Program at the Auke Bay Laboratories of the Alaska Fisheries Science
Center.
NR 53
TC 6
Z9 6
U1 0
U2 14
PU ARCTIC INST N AMER
PI CALGARY
PA UNIV OF CALGARY 2500 UNIVERSITY DRIVE NW 11TH FLOOR LIBRARY TOWER,
CALGARY, ALBERTA T2N 1N4, CANADA
SN 0004-0843
J9 ARCTIC
JI Arctic
PD SEP
PY 2013
VL 66
IS 3
BP 257
EP 268
PG 12
WC Environmental Sciences; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 230AR
UT WOS:000325309500002
ER
PT J
AU Owens, BAM
Stahl, MT
Corron, NJ
Blakely, JN
Illing, L
AF Owens, Benjamin A. M.
Stahl, Mark T.
Corron, Ned J.
Blakely, Jonathan N.
Illing, Lucas
TI Exactly solvable chaos in an electromechanical oscillator
SO CHAOS
LA English
DT Article
ID BEHAVIOR; EQUATION; DYNAMICS
AB A novel electromechanical chaotic oscillator is described that admits an exact analytic solution. The oscillator is a hybrid dynamical system with governing equations that include a linear second order ordinary differential equation with negative damping and a discrete switching condition that controls the oscillatory fixed point. The system produces provably chaotic oscillations with a topological structure similar to either the Lorenz butterfly or Rossler's folded-band oscillator depending on the configuration. Exact solutions are written as a linear convolution of a fixed basis pulse and a sequence of discrete symbols. We find close agreement between the exact analytical solutions and the physical oscillations. Waveform return maps for both configurations show equivalence to either a shift map or tent map, proving the chaotic nature of the oscillations. (C) 2013 AIP Publishing LLC.
C1 [Owens, Benjamin A. M.] Duke Univ, Dept Mech Engn & Mat Sci, Durham, NC 27708 USA.
[Stahl, Mark T.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Corron, Ned J.; Blakely, Jonathan N.] US Army, Res Dev & Engn Command, Redstone Arsenal, AL 35898 USA.
[Illing, Lucas] Reed Coll, Dept Phys, Portland, OR 97202 USA.
RP Owens, BAM (reprint author), Duke Univ, Dept Mech Engn & Mat Sci, Durham, NC 27708 USA.
EM benjamin.owens@duke.edu
OI Corron, Ned/0000-0002-3232-5024
NR 20
TC 7
Z9 7
U1 0
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1054-1500
J9 CHAOS
JI Chaos
PD SEP
PY 2013
VL 23
IS 3
AR 033109
DI 10.1063/1.4812723
PG 9
WC Mathematics, Applied; Physics, Mathematical
SC Mathematics; Physics
GA 228AW
UT WOS:000325158300009
PM 24089945
ER
PT J
AU Shi, Y
Li, KF
Yung, YL
Aumann, HH
Shi, ZQ
Hou, TY
AF Shi, Yuan
Li, King-Fai
Yung, Yuk L.
Aumann, Hartmut H.
Shi, Zuoqiang
Hou, Thomas Y.
TI A decadal microwave record of tropical air temperature from AMSU-A/aqua
observations
SO CLIMATE DYNAMICS
LA English
DT Article
DE Atmospheric variability; Principal mode decomposition; Adaptive
analysis; Amplitude and phase profiles; Near-annual variability;
Temperature trends
ID QUASI-BIENNIAL OSCILLATION; SEA-SURFACE TEMPERATURE; ANNUAL CYCLE;
CLIMATE-CHANGE; TROPOPAUSE TEMPERATURES; SEMIANNUAL OSCILLATION;
SOUTHERN OSCILLATION; MIDDLE ATMOSPHERE; HILBERT SPECTRUM; EL-NINO
AB Atmospheric temperature is one of the most important climate variables. This observational study presents detailed descriptions of the temperature variability imprinted in the 9-year brightness temperature data acquired by the Advanced Microwave Sounding Unit-Instrument A (AMSU-A) aboard Aqua since September 2002 over tropical oceans. A non-linear, adaptive method called the Ensemble Joint Multiple Extraction has been employed to extract the principal modes of variability in the AMSU-A/Aqua data. The semi-annual, annual, quasi-biennial oscillation (QBO) modes and QBO-annual beat in the troposphere and the stratosphere have been successfully recovered. The modulation by the El Nio/Southern oscillation (ENSO) in the troposphere was found and correlates well with the Multivariate ENSO Index. The long-term variations during 2002-2011 reveal a cooling trend (-0.5 K/decade at 10 hPa) in the tropical stratosphere; the trend below the tropical tropopause is not statistically significant due to the length of our data. A new tropospheric near-annual mode (period similar to 1.6 years) was also revealed in the troposphere, whose existence was confirmed using National Centers for Environmental Prediction Reanalysis air temperature data. The near-annual mode in the troposphere is found to prevail in the eastern Pacific region and is coherent with a near-annual mode in the observed sea surface temperature over the Warm Pool region that has previously been reported. It remains a challenge for climate models to simulate the trends and principal modes of natural variability reported in this work.
C1 [Shi, Yuan] Univ Hong Kong, Dept Phys, Pokfulam, Hong Kong, Peoples R China.
[Li, King-Fai; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Aumann, Hartmut H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Shi, Zuoqiang; Hou, Thomas Y.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Li, KF (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM kfl@gps.caltech.edu
OI Li, King-Fai/0000-0003-0150-2910
FU Overseas Research Fellowship of the Faculty of Science and Department of
Physics, The University of Hong Kong
FX We thank Dr. Dong L. Wu for critical comments and two anonymous referees
for constructive criticisms that improved this paper. YS was supported
by Overseas Research Fellowship of the Faculty of Science and Department
of Physics, The University of Hong Kong. The extraction of the
AMSU-A/Aqua data from the Atmospheric InfraRed Spectrometer
(AIRS)/AMSU-A data archive was supported by a research grant
administered by Dr. Ramesh Kakar, EOS Aqua Programme Scientist at NASA
Headquarter and the Keck Institute for Space Studies at California
Institute of Technology. We also thank Dr. Thomas Hearty for
proofreading our paper and sharing his results on AIRS data. The TMI SST
data were downloaded from ftp://ssmi.com/tmi/. The standardized zonal
winds at 30 and 50 hPa (u30hPa and u50hPa) were
downloaded from http://www.cpc.ncep.noaa.gov/data/indices/. The MEI
index for ENSO was downloaded from
http://www.esrl.noaa.gov/psd/enso/mei/. YLY designed the approach; HHA
provided the monthly-averaged AMSU-A/Aqua data; TYH and ZS provided the
DMP package; ZS and YS developed the EJME package; YS performed the time
series decomposition; KFL, YLY, and YS interpreted the results and wrote
most of the manuscript.
NR 63
TC 1
Z9 1
U1 3
U2 12
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 SEP
PY 2013
VL 41
IS 5-6
BP 1385
EP 1405
DI 10.1007/s00382-013-1696-x
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 226YO
UT WOS:000325073700016
ER
PT J
AU Jolivet, R
Lasserre, C
Doin, MP
Peltzer, G
Avouac, JP
Sun, J
Dailu, R
AF Jolivet, R.
Lasserre, C.
Doin, M. -P.
Peltzer, G.
Avouac, J-P
Sun, J.
Dailu, R.
TI Spatio-temporal evolution of aseismic slip along the Haiyuan fault,
China: Implications for fault frictional properties
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE shallow creep; strike-slip fault; Tibet; SAR interferometry; frictional
properties
ID SAN-ANDREAS FAULT; GLOBAL POSITIONING SYSTEM; HAYWARD FAULT; POSTSEISMIC
DEFORMATION; GEODETIC MEASUREMENTS; CENTRAL CALIFORNIA; LARGE
EARTHQUAKES; OKI EARTHQUAKE; EASTERN TAIWAN; SURFACE CREEP
AB We use 20 years of Synthetic Aperture Radar acquisitions by the ERS and Envisat satellites to investigate the spatial and temporal variations of strain rates along the 35-km long creeping section of the Haiyuan fault, at the north eastern boundary of the Tibetan plateau. We then use the derived displacements to infer the fault's frictional properties and discuss the relationship between creep and the seismic behavior of the fault. Located in between a millennial seismic gap and the 1920 M8 surface rupture trace, this section has an average creep rate of 5 +/- 1 mm/yr, about the interseismic loading rate. The comparison of average surface velocity profiles derived from SAR interferometry across the creeping section reveals a creep rate increase and/or a creep migration to shallower depth between the 1990s and the 2000s. We apply a smoothed time series analysis scheme on Envisat InSAR data to investigate the creep rate variations during the 2004-2009 time period. Our analysis reveals that the creep rate accelerated in 2007, although data resolution does not allow to better constrain the onset of creep acceleration and its amplitude. Both decadal and short term transient behaviors are coeval with the largest earthquakes (M similar to 4-5) along the fault segment in recent years. From the precise mapping of the surface fault trace, we use the fault strike variations and the Mohr circle construction to compute the along-strike distribution of the friction coefficient along the creeping segment and compare it with the observed distribution of the creep rate. We find that the creep rate scales logarithmically with the friction coefficient, in agreement with the rate-and-state friction law in a rate strengthening regime. The estimated value of delta mu/delta log V similar to 2 x 10(-3) indicates that the earthquakes occurring along the creeping section cannot be the cause for a significant change in the overall segment's creep rate and that the recorded micro seismicity is most likely creep-driven. Finally, given the size and frictional properties of the creeping section, we estimate, based on previous models of dynamic rupture simulations, a 0-20% probability for a rupture to break through this section. Together with the geometrical configuration of the Haiyuan fault, these results suggest that the creeping segment may act as a persistent barrier to earthquake propagation. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Jolivet, R.; Lasserre, C.; Doin, M. -P.] Univ Grenoble 1, CNRS, Inst Sci Terre ISTerre, UMR 5275, F-38041 Grenoble, France.
[Peltzer, G.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Peltzer, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Avouac, J-P] CALTECH, Tecton Observ, Pasadena, CA 90125 USA.
[Dailu, R.] Chinese Earthquake Adm, Lanzhou Seismol Inst, Lanzhou, Peoples R China.
[Sun, J.] Chinese Earthquake Adm, Inst Geol, Beijing, Peoples R China.
RP Jolivet, R (reprint author), CALTECH, Tecton Observ, Pasadena, CA 90125 USA.
EM rjolivet@caltech.edu
RI Avouac, Jean-Philippe/B-5699-2015; Lasserre, Cecile/D-7073-2017
OI Avouac, Jean-Philippe/0000-0002-3060-8442; Lasserre,
Cecile/0000-0002-0582-0775
FU French "Extraction et Fusion d'Information et de Donnees
d'Interferometrie Radar" program (EFIDIR, ANR, France); Programme
National de Teledetection Spatiale (CNES); Gordon and Betty Moore
Foundation [GBMF 423.01]
FX The SAR data set was provided by the European Space Agency (ESA) in the
framework of the Dragon 2 program (ID 2509 and 5305). This program also
supported R. Jolivet's work, through the Young Scientist fellowship.
Funding was provided by the French "Extraction et Fusion d'Information
et de Donnees d'Interferometrie Radar" program (EFIDIR, ANR, France) and
Programme National de Teledetection Spatiale (CNES). Part of G.
Peltzer's contribution was done at the Jet Propulsion Laboratory,
California Institute of Technology under contract with NASA. This
research was partially funded by the Gordon and Betty Moore Foundation
through Grant GBMF 423.01 to the Tectonics Observatory. This Tectonics
Observatory contribution #234. Figures and map were prepared using
Generic Mapping Tools software (Wessel and Smith, 1995).
NR 89
TC 23
Z9 23
U1 4
U2 37
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 SEP
PY 2013
VL 377
BP 23
EP 33
DI 10.1016/j.eps1.2013.07.020
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 228MY
UT WOS:000325192100003
ER
PT J
AU Jones, SM
Anderson, MS
Dominguez, G
Tsapin, A
AF Jones, S. M.
Anderson, M. S.
Dominguez, G.
Tsapin, A.
TI Thermal calibrations of hypervelocity capture in aerogel using magnetic
iron oxide particles
SO ICARUS
LA English
DT Article
DE Impact processes; Comets; Comets, Coma
ID COMET 81P/WILD-2 DUST; FORCE MICROSCOPY; SILICA AEROGEL; STARDUST;
IMPACT; COLLECTION; TRACKS
AB Due to its extremely high porosity and the nanoscale filaments that make up its structure, aerogel is an excellent material for the capture of hypervelocity, micron-sized particles. A great deal of the kinetic energy of a particle is converted to thermal energy during the capture process, altering or even destroying components of the particle. The studies described here were conducted using aggregate projectiles made up of magnetic sub-micron hematite particles in an attempt to directly measure the temperatures experienced by fine particles during hypervelocity capture in aerogels. When these particles are heated to a temperature above their Curie temperature (675 degrees C) during the capture, they lose their magnetization. Thus, by impact testing these particles in aerogels at different velocities, we were able to determine if individual components of these aggregate particles were heated to a temperature greater than their Curie temperature by observing their magnetization. After impact testing, the particles were extracted from the aerogel, thin sectioned, and observed using atomic and magnetic force microscopy, as well as, electron paramagnetic resonance. Terminal particles for impacts at or above 4.5 km/s were still magnetic, while those from the track walls were not. Even terminal particles captured at 6.6 km/s were still magnetic. Iron oxide particles coated with silica, to mimic extraterrestrial materials, from track walls captured at 5.47 km/s were still magnetic. The study also demonstrated that aggregate projectiles can survive the forces they are subjected to during hypervelocity launch in a light gas gun. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Jones, S. M.; Anderson, M. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dominguez, G.] Calif State Univ San Marcos, Dept Phys, San Marcos, CA 92096 USA.
[Tsapin, A.] Univ Calif Riverside, Riverside, CA 92521 USA.
RP Jones, SM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 125-109, Pasadena, CA 91109 USA.
EM Steven.M.Jones@jpl.nasa.gov
FU NASA Science Mission Directorate, Planetary Science Division;
NationalAeronautics and Space Administration
FX We thank M. Burchell (University of Kent) for conducting the 6.6 km/s
impact test and R. Mielke at JPL for assistance in embedding and
microtoming the captured particles. S.M.J. and M.S.A. thank the NASA
Science Mission Directorate, Planetary Science Division for providing
the funding to conduct this work. This research was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the NationalAeronautics and Space Administration.
Copyright statement must be added until copyright is transferred to
publisher. Copyright 2013. All rights reserved.
NR 31
TC 2
Z9 2
U1 1
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
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 1
EP 9
DI 10.1016/j.icarus.2013.05.015
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200001
ER
PT J
AU Kreslavsky, MA
Head, JW
Neumann, GA
Rosenburg, MA
Aharonson, O
Smith, DE
Zuber, MT
AF Kreslavsky, Mikhail A.
Head, James W.
Neumann, Gregory A.
Rosenburg, Margaret A.
Aharonson, Oded
Smith, David E.
Zuber, Maria T.
TI Lunar topographic roughness maps from Lunar Orbiter Laser Altimeter
(LOLA) data: Scale dependence and correlation with geologic features and
units
SO ICARUS
LA English
DT Article
DE Moon, surface; Regoliths; Data reduction techniques; Geological
processes
ID INNER SOLAR-SYSTEM; EARTH-MOON SYSTEM; CRATER CHAINS; ARISTARCHUS
REGION; TIDAL DISRUPTION; MARS; STRATIGRAPHY; SURFACE; AGES; EVOLUTION
AB We present maps of the topographic roughness of the Moon at hectometer and kilometer scales. The maps are derived from range profiles obtained by the Lunar Orbiter Laser Altimeter (LOLA) instrument onboard the Lunar Reconnaissance Orbiter (LRO) spacecraft. As roughness measures, we used the interquartile range of profile curvature at several baselines, from 115 m to 1.8 km, and plotted these in a global map format. The maps provide a synoptic overview of variations of typical topographic textures and utilize the exceptional ranging precision of the LOLA instrument. We found that hectometer-scale roughness poorly correlates with kilometer-scale roughness, because they reflect different sets of processes and time scales. Hectometer-scale roughness is controlled by regolith accumulation and modification processes and affected by the most recent events, primarily, geologically recent (1-2 Ga) meteoritic impacts. Kilometer-scale roughness reflects major geological (impact, volcanic and tectonic) events in earlier geological history. Young large impact craters are rough, and their roughness decreases with age. The global roughness maps revealed a few unusually dense clusters of hectometer- and decameter-size impact craters that differ in their morphology and settings from typical secondary crater clusters and chains; the origin of these features is enigmatic. The maps can assist in the geological mapping of the lunar maria by revealing contacts between volcanic plain units. The global roughness maps also clearly reveal cryptomaria, old volcanic plains superposed by younger materials, primarily crater and basin ejecta. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Kreslavsky, Mikhail A.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Rosenburg, Margaret A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Aharonson, Oded] Weizmann Inst Sci, Ctr Planetary Sci, IL-76100 Rehovot, Israel.
[Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Kreslavsky, MA (reprint author), Univ Calif Santa Cruz, 1156 High St, Santa Cruz, CA 95064 USA.
EM mkreslav@ucsc.edu
RI Neumann, Gregory/I-5591-2013; Kreslavsky, Mikhail/J-3425-2013;
OI Neumann, Gregory/0000-0003-0644-9944; Kreslavsky,
Mikhail/0000-0002-1900-826X
FU NASA Lunar Reconnaissance Orbiter Lunar Orbiter Laser Altimeter (LOLA)
experiment [NNX09AM54G, NNX11AK29G]; NASA Lunar Science Institute
FX Discussions with Yuriy Shkuratov and Erik Asphaug were helpful. We
acknowledge financial support from the NASA Lunar Reconnaissance Orbiter
Lunar Orbiter Laser Altimeter (LOLA) experiment (NNX09AM54G and
NNX11AK29G to J.W.H.) and the NASA Lunar Science Institute.
NR 49
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U1 0
U2 20
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 52
EP 66
DI 10.1016/j.icarus.2013.04.027
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200006
ER
PT J
AU Besse, S
Yokota, Y
Boardman, J
Green, R
Haruyama, J
Isaacson, P
Mall, U
Matsunaga, T
Ohtake, M
Pieters, C
Staid, M
Sunshine, J
Yamamoto, S
AF Besse, S.
Yokota, Y.
Boardman, J.
Green, R.
Haruyama, J.
Isaacson, P.
Mall, U.
Matsunaga, T.
Ohtake, M.
Pieters, C.
Staid, M.
Sunshine, J.
Yamamoto, S.
TI One Moon, many measurements 2: Photometric corrections
SO ICARUS
LA English
DT Article
DE Moon, Surface; Photometry; Spectroscopy
ID KAGUYA MULTIBAND IMAGER; MINERALOGY MAPPER M-3; SELENE; REFLECTANCE;
CALIBRATION; CHANDRAYAAN-1; IRRADIANCE; ALBEDO
AB Observations of the lunar surface within the past 10 years have been made with various lunar remote sensing instruments, the Moon Mineralogy Mapper (M-3) onboard the Chandrayaan-1 mission, the Spectral Profiler (SP), the Multiband Imager (MI), the Terrain Camera (TC) onboard the SELENE mission, and the ground based USGS Robotic Lunar Observatory (ROLO) for some of them. The lunar phase functions derived from these datasets, which are used in the photometric modeling to correct for the various illumination conditions of the data, are compared to assess their differences and similarity in order to improve interpretations of lunar surface spectra. The phase functions are found to be similar across various phase angles except in the 0-20 degrees range. Differences across the 0-20 degrees range likely result from two different inputs in the photometric modeling of the M-3 and SP data: (I) M-3 has larger emission angles due to the characteristics of the instrument and the attitude of the spacecraft, and (2) M-3 viewing geometry was derived from the local topography whereas SP used a spherical Moon (no topography). The combination of these two different inputs affects the phase function at small phase angles where shadows play a more substantial role, with spatial resolution differences between M-3 and SP being another possible source for the differences. SP data are found to be redder (i.e., steeper slope with increasing wavelengths) than MI, M-3 and ROLO. Finally, the M-3 overall reflectance is also found to be lower than that the other instruments (i.e., MI, SP, and ROLO), generally at least 10% darker than MI. These differences can be observed at local scales in specific examples at hundreds of meters resolutions. At regional and global scales, the same differences are found, which demonstrates the overall stability of the various datasets. The observations from M-3, TC, SP and MI are very stable and agree well; however caution should be used when making interpretations based on the spectral slope of SP data or on the absolute reflectance of M-3 data. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Besse, S.] ESA, ESTEC, Noordwijk, Netherlands.
[Yokota, Y.; Matsunaga, T.; Yamamoto, S.] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan.
[Boardman, J.] Analyt Imaging & Geophys LLC, Boulder, CO 80303 USA.
[Green, R.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Haruyama, J.; Ohtake, M.] Japan Aerosp Explorat Agcy, Sagamihara, Kanagawa, Japan.
[Isaacson, P.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Mall, U.] Max Planck Inst Solar Syst Res, Lindau, Germany.
[Pieters, C.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Staid, M.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Sunshine, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Besse, S (reprint author), ESA, ESTEC, Keplerlaan 1, Noordwijk, Netherlands.
EM sbesse@rssd.esa.int
OI Besse, Sebastien/0000-0002-1052-5439
FU NASA
FX The M3 instrument was funded as a mission of opportunity
through the NASA Discovery program. The M3 team is grateful
to ISRO for the opportunity to fly as a guest instrument on
Chandrayaan-1. The authors would also like to thank Fujitsu Ltd.,
Fujinon Corporation, JASCO Corporation, and Mitsubishi Space Software
Company, Ltd., for their dedicated efforts in developing LISM and its
ground data system. We acknowledge P. Pinet and an anonymous reviewer
for helpful comments that improved the quality and clarity of the
manuscript. This is HIGP publication number 2011, SOEST publication
number 8924.
NR 36
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 127
EP 139
DI 10.1016/j.icarus.2013.05.009
PG 13
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SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200013
ER
PT J
AU Zhang, X
West, RA
Banfield, D
Yung, YL
AF Zhang, X.
West, R. A.
Banfield, D.
Yung, Y. L.
TI Stratospheric aerosols on Jupiter from Cassini observations
SO ICARUS
LA English
DT Article
DE Jupiter, Atmosphere; Photometry; Radiative transfer; Atmospheres,
Structure
ID INDUCED INFRARED-SPECTRA; H-2-HE PAIRS; VERTICAL DISTRIBUTIONS; HAZE
FORMATION; ATMOSPHERE; TEMPERATURES; SCATTERING; MODEL;
SPECTROPHOTOMETRY; EQUATORIAL
AB We retrieved global distributions and optical properties of stratospheric aerosols on Jupiter from ground-based NIR spectra and multiple-phase-angle images from Cassini Imaging Science Subsystem (ISS). A high-latitude haze layer is located at similar to 10-20 mbar, higher than in the middle and low latitudes (similar to 50 mbar). Compact sub-micron particles are mainly located in the low latitudes between 40 degrees S and 25 degrees N with the particle radius between 0.2 and 0.5 mu m. The rest of the stratosphere is covered by the particles known as fractal aggregates. In the nominal case with the imaginary part of the UV refractive index 0.02, the fractal aggregates are composed of about a thousand 10-nm-size monomers. The column density of the aerosols at pressure less than 100 mbar ranges from similar to 10(7) cm(-2) at low latitudes to similar to 10(9) cm(-2) at high latitudes. The mass loading of aerosols in the stratosphere is similar to 10(-6) g cm(-2) at low latitudes to similar to 10(-4) g cm(-2) in the high latitudes. Multiple solutions due to the uncertainty of the imaginary part of the refractive index are discussed. The stratospheric haze optical depths increase from similar to 0.03 at low latitudes to about a few at high latitudes in the UV wavelength (similar to 0.26 mu m), and from similar to 0.03 at low latitudes to similar to 0.1 at high latitudes in the NIR wavelength (similar to 0.9 mu m). (C) 2013 Elsevier Inc. All rights reserved.
C1 [Zhang, X.; Yung, Y. L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Zhang, X.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Zhang, X.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[West, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Banfield, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Zhang, X (reprint author), Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
EM xiz@lpl.arizona.edu
OI Banfield, Don/0000-0003-2664-0164
FU Outer Planets Research program via NASA [JPL 1452240]; NASA
[NNX09AB72G]; Bisgrove Scholar Program in the University of Arizona
FX We thank M. Lemmon for the parameterization model for the aggregated
particles, T. Dowling for the C-DISORT program, P.G. Irwin for the
CH4 correlated-k coefficients, M. Line for helpful
discussions, and K. Rages and the other reviewer for useful comments.
This research was supported by the Outer Planets Research program via
NASA Grant JPL 1452240 to the California Institute of Technology. Y.L.Y.
was supported in part by NASA NNX09AB72G grant to the California
Institute of Technology. X.Z. was supported in part by the Bisgrove
Scholar Program in the University of Arizona.
NR 39
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 159
EP 171
DI 10.1016/j.icarus.2013.05.020
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200015
ER
PT J
AU Potter, AE
Killen, RM
Reardon, KP
Bida, TA
AF Potter, A. E.
Killen, R. M.
Reardon, Kevin P.
Bida, T. A.
TI Observation of neutral sodium above Mercury during the transit of
November 8, 2006
SO ICARUS
LA English
DT Article
DE Mercury, atmosphere; Abundances, atmospheres; Atmospheres structure
ID EXOSPHERE; PROFILES; EMISSION; FLYBY; MODEL; MOON; IBIS
AB We mapped the absorption of sunlight by sodium vapor in the exosphere of Mercury during the transit of Mercury on November 8, 2006, using the IBIS Interferometric BIdimensional Spectrometer at the Dunn Solar Telescope operated by the National Solar Observatory at Sunspot, New Mexico. The measurements were reduced to line-of-sight equivalent widths for absorption at the sodium D-2 line around the shadow of Mercury. The sodium absorption fell off exponentially with altitude up to about 600 km. However there were regions around north and south polar-regions where relatively uniform sodium absorptions extended above 1000 km. We corrected the 0-600 km altitude profiles for seeing blur using the measured point spread function. Analysis of the corrected altitude distributions yielded surface densities, zenith column densities, temperatures and scale heights for sodium all around the planet. Sodium absorption on the dawn side equatorial terminator was less than on the dusk side, different from previous observations of the relative absorption levels. We also determined Earthward velocities for sodium atoms, and line widths for the absorptions. Earthward velocities resulting from radiation pressure on sodium averaged 0.8 km/s, smaller than a prediction of 1.5 km/s. Most line widths were in the range of 20 mA after correction for instrumental broadening, corresponding to temperatures in the range of 1000 K. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Potter, A. E.] Natl Solar Observ, Tucson, AZ 85719 USA.
[Killen, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Reardon, Kevin P.] INAF Arcetri Astrophys Observ, Florence, Italy.
[Reardon, Kevin P.] Natl Solar Observ, Sunspot, NM 88349 USA.
[Bida, T. A.] Lowell Observ, Flagstaff, AZ 86001 USA.
RP Potter, AE (reprint author), Natl Solar Observ, Tucson, AZ 85719 USA.
EM apotter@noao.edu; rosemary.killen@nasa.gov; kreardon@nso.edu;
tbida@lowell.edu
FU NASA under MESSENGER Participating Scientist Program; NASA
FX The National Solar Observatory is operated by the Association of
Universities for Research in Astronomy under a cooperative agreement
with the National Science Foundation. The IBIS instrument used for the
transit observations at Sunspot, New Mexico, was built by the Arcetri
Astrophysical Observatory and the Department of Astronomy and Space
Science of the Florence University, in collaboration with the Department
of Physics of the Roma "Tor Vergata" University. We thank the Community
Coordinated Modeling Center (CCMC) at NASA Goddard Space Flight Center
for running the ENLIL model to estimate the solar wind and
interplanetary magnetic field parameters at the time of our
observations. RMK acknowledges support from NASA under the MESSENGER
Participating Scientist Program and NASA Planetary Astronomy grants. We
also thank Jay Pasachoff, Bryce Babcock of Williams College, as well as
Fabio Cavallini and Antonio Vecchio of Arcetri Observatory, for their
assistance in planning the observations. We are very grateful to Doug
Gilliam, Mike Bradford, and Joe Elrod and the NSO staff for all their
outsized efforts in preparing for and carrying out the observations at
Sunspot, New Mexico. We thank Claude Plymate, Eric Galayda and Matthew
Knight for supporting the transit observations that were made with the
McMath-Pierce Solar Telescope at Kitt Peak, Arizona, using the Main
Spectrograph. We also thank the reviewers, who provided insightful
comments that improved the quality of this paper.
NR 41
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 172
EP 185
DI 10.1016/j.icarus.2013.05.029
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200016
ER
PT J
AU Urata, RA
Toon, OB
AF Urata, Richard A.
Toon, Owen B.
TI Simulations of the martian hydrologic cycle with a general circulation
model: Implications for the ancient martian climate
SO ICARUS
LA English
DT Article
DE Mars; Mars, Atmosphere; Mars, Climate
ID WATER-ICE CLOUDS; RADIATIVE-TRANSFER; EARLY MARS; ATMOSPHERIC
OBSERVATIONS; TROPICAL TROPOPAUSE; PREDICTION SCHEME; CIRRUS CLOUDS;
HEATING RATES; VAPOR; PRECIPITATION
AB We use a general circulation model (Urata, R.A., Toon, O.B. [2013]. Icarus, submitted for publication) to simulate the martian hydrologic cycle, including the radiative effects of water-ice clouds. We find that the current observed hydrologic cycle can be duplicated by tuning the polar cap albedo. The hydrologic cycle is very sensitive to the size and albedo of the North Polar water-ice cap. The radiative effects of ice clouds on atmospheric temperatures can be significant. Simulations of an ancient climate were performed with a 500 mb CO2 atmosphere and a reduced solar constant. The results show that the climate is highly sensitive to the hydrologic cycle, and can range from cold and dry, to warm and wet depending on initial conditions, cloud particle size, precipitation rates, and cloud cover fraction. A warm climate is obtained by assuming cloud ice particles greater than or equal to 10 gm, and by reducing the efficiency of precipitation to maximize the cloud optical thicknesses. The warm, wet climates have precipitation rates that are 10% of the present day Earth. While carbon dioxide plays only a minor role in creating warm temperatures, it is necessary to have more than 250 mb of carbon dioxide in order to obtain these high temperatures for the conditions assumed in our simulations due to the need for heat transport to the poles. Published by Elsevier Inc.
C1 [Urata, Richard A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Toon, Owen B.] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Toon, Owen B.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
RP Urata, RA (reprint author), NASA, Ames Res Ctr, Bldg N245,Room 207, Moffett Field, CA 94035 USA.
EM richard.urata@colorado.edu
FU NASA [NNX08AV46H]
FX This research was funded by NASA Graduate Student Research Program
fellowship NNX08AV46H.
NR 81
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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 SEP-OCT
PY 2013
VL 226
IS 1
BP 229
EP 250
DI 10.1016/j.icarus.2013.05.014
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200020
ER
PT J
AU Clancy, RT
Sandor, BJ
Garcia-Munoz, A
Lefevre, F
Smith, MD
Wolff, MJ
Montmessin, F
Murchie, SL
Nair, H
AF Clancy, R. Todd
Sandor, Brad J.
Garcia-Munoz, Antonio
Lefevre, Franck
Smith, Michael D.
Wolff, Michael J.
Montmessin, Franck
Murchie, Scott L.
Nair, Hari
TI First detection of Mars atmospheric hydroxyl: CRISM Near-IR measurement
versus LMD GCM simulation of OH Meinel band emission in the Mars polar
winter atmosphere
SO ICARUS
LA English
DT Article
DE Mars, Atmosphere; Aeronomy; Photochemistry; Spectroscopy; Atmospheres,
Dynamics
ID VENUS EXPRESS OBSERVATIONS; MARTIAN ATMOSPHERE; PHOTOCHEMICAL MODEL;
NIGHTGLOW; HYDROGEN; SPECTROSCOPY; CHEMISTRY; AIRGLOW; METHANE; SPICAM
AB Visible and near-IR Meinel band emissions originate from excited OH in the terrestrial upper atmosphere (Meinel, I.A.B. [1950]. Astrophys. J. 111, 555. http://dx.doi.org/10.1086/145296), and have recently been detected in the Venus nightside upper mesosphere (Piccioni, G. et al. [2008]. Astron. Astrophys. 483, L29-L33. http://dx.doi.org/10.1051/0004-6361:200809761). Meinel band observations support key studies of transport and photochemistry in both of these atmospheres. In the case of Mars, OH regulates the basic stability of the CO2 atmosphere to photolytic decomposition (to CO and O-2, e.g. Parkinson, T.D., Hunten, D.M. [1972]. J. Atmos. Sci. 29, 1380-1390. http://dx.doi.org/10.1175/1520-0469(1972) 029<1380:SAAOOO>2.0.CO;2), and yet has never been measured. We present the first detection of Mars atmospheric OH, associated with CRISM near-IR spectral limb observations of polar night Meinel band emissions centered at 1.45 and 2.9 mu m. Meinel band (1-0), (2-1), and (2-0) average limb intensities of 990 +/- 280, 1060 +/- 480, and 200 +/- 100 kiloRayleighs (kR), respectively, are determined for 70-90 NS polar winter latitudes over altitudes of 40-56 km. Additional OH bands, such as (3-2), (3-1), and (4-2), present <= 1 sigma measurements. Uncertainty in the (4-2) band emission rate contributes to increased uncertainty in the determination of the O-2((1)Delta(g)) (0-0)/(0-1) band emission ratio (A(00)/A(01) = 47(-12)(+26)). An average profile retrieval for Mars OH polar nightglow indicates 45-55 km altitude levels for volume emission rates (VER) of 0.4 (2-0) to 2 (1-0, 2-1) x 10(4) photons/(cm(3) s). Similar to polar night O-2((1)Delta(g)) emission (e.g. Clancy, R.T. et al. [2012]. J. Geophys. Res. (Planets) 117, E00J10. http://dx.doi.org/10.1029/2011JE004018), Meinel OH band emission is supported by upper level, winter poleward transport of O and H in the deep Hadley solsticial circulations of Mars. The retrieved OH emission rates are compared to polar winter OH nightglow simulated by the LMD (Laboratoire de Meteorologie Dynamique) photochemical GCM (global climate model), employing detailed photochemistry (e.g. Lefevre, F., Lebonnois, S., Montmessin, F., Forget, F. [2004]. J. Geophys. Res. (Planets) 109, E07004. http://dx.doi.org/10.1029/2004JE002268) and energy transfer processes (excitation and quenching) developed for Mars Meinel OH band nightglow by Garcia Munoz et al. (Garcia Munoz, A., McConnell, J.C., McDade, I.C., Melo, S.M.L. [2005]. Icarus 176, 75-95). Modeled versus observed OH emission behavior agrees within measurement uncertainties with the assumptions of a Bates-Nicolet (H + O-3) source for excited OH production, and 'collisional-cascade' quenching of the OH vibrational population by CO2. 'Sudden-death' quenching of excited OH by CO2 leads to 100x less OH emission than observed. The combined agreement between LMD GCM simulated and CRISM observed O-2((1)Delta(g)) and Meinel OH polar nightglow behaviors represents a significant demonstration of the LMD model capability to couple odd oxygen and hydrogen photochemistry and transport by the Mars global circulation in a realistic fashion. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Clancy, R. Todd; Sandor, Brad J.; Wolff, Michael J.] Space Sci Inst, Boulder, CO 80301 USA.
[Garcia-Munoz, Antonio] ESA, RSSD, ESTEC, NL-2200 AG Noordwijk, Netherlands.
[Lefevre, Franck; Montmessin, Franck] UPMC Univ Paris, CNRS, LATMOS, Paris, France.
[Smith, Michael D.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Murchie, Scott L.; Nair, Hari] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Clancy, RT (reprint author), Space Sci Inst, Boulder, CO 80301 USA.
EM clancy@spacescience.org
RI Murchie, Scott/E-8030-2015
OI Murchie, Scott/0000-0002-1616-8751
FU NASA [NNX10AL61G]
FX We are indebted to the excellent MRO and CRISM operations staff for the
collection and processing of CRISM limb observations presented here.
Grant support for this work was provided by the NASA MDAP Program (under
NASA Contract Award Number NNX10AL61G).
NR 55
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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 SEP-OCT
PY 2013
VL 226
IS 1
BP 272
EP 281
DI 10.1016/j.icarus.2013.05.035
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200024
ER
PT J
AU Spilker, L
Ferrari, C
Morishima, R
AF Spilker, Linda
Ferrari, Cecile
Morishima, Ryuji
TI Saturn's ring temperatures at equinox
SO ICARUS
LA English
DT Article
DE Saturn, Rings; Infrared observations; Radiative transfer
ID THERMAL INFRARED-EMISSION; SELF-GRAVITY WAKES; CASSINI CIRS; MULTILAYER
MODEL; PLANETARY RINGS; BENDING WAVES; C-RING; PARTICLES; SIMULATIONS;
ROTATION
AB Modeling the thermal emission of Saturn's rings is challenging due to the numerous heating sources as well as the structural properties of the disk and of the particles that are closely related. At equinox, however, rings are externally heated by Saturn alone and the problem is somewhat simplified. We test the abilities of our current models to reproduce the temperatures observed with the Cassini-CIRS instrument around equinox in August 2009. A simple semi-analytic model with the mutual shadowing effect can mostly explain the radial profile of the equinox ring temperatures, except the model predicts lower temperatures than those observed for the A ring. The temperature variation at a given saturnocentric radius is primarily caused by observational geometry variations relative to Saturn. The observed temperature increases with decreasing Saturn-ring-observer angle. In addition, we found evidence that the leading hemispheres of particles are warmer than the trailing hemispheres at least for the C ring and probably for the A and B rings as well. This is explained if some fraction of particles has spin rates lower than the synchronous rotation rate as predicted by N-body simulations. The spin model for a monolayer ring (Ferrari, C., Leyrat, C. [2006]. Astron. Astrophys. 447, 745-760) can fit the temperature variations with spacecraft longitude observed in the C ring with currently known thermal properties and a mixing of slow and fast rotators. The multilayer model (Morishima, R., Salo, H., Ohtsuki, K. [2009]. Icarus 201, 634-654) can reproduce the temperatures of the B and C rings but gives A ring temperatures that are significantly lower than those observed as does the simple semi-analytic model. More advanced models which take into account self-gravity wakes may explain the A ring temperature behavior. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Spilker, Linda; Morishima, Ryuji] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ferrari, Cecile] Univ Paris Diderot, Lab AIM Paris Saclay, CEA, Irfu CNRS,INSU, F-91191 Gif Sur Yvette, France.
[Morishima, Ryuji] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
RP Spilker, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Linda.J.Spilker@jpl.nasa.gov
RI Ferrari, Cecile/P-9735-2016
OI Ferrari, Cecile/0000-0001-5962-7439
FU NASA; Centre National d'Etudes Spatiales (CNES); Commissariat a
l'Energie Atomique et aux Energies Alternative
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. Government
sponsorship acknowledged. This work was also supported by the NASA's
Cassini Data Analysis program. C. Ferrari acknowledges the support by
the Centre National d'Etudes Spatiales (CNES) and the Commissariat a
l'Energie Atomique et aux Energies Alternative.
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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 SEP-OCT
PY 2013
VL 226
IS 1
BP 316
EP 322
DI 10.1016/j.icarus.2013.06.002
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200027
ER
PT J
AU Naidu, SP
Margot, JL
Busch, MW
Taylor, PA
Nolan, MC
Brozovic, M
Benner, LAM
Giorgini, JD
Magri, C
AF Naidu, Shantanu P.
Margot, Jean-Luc
Busch, Michael W.
Taylor, Patrick A.
Nolan, Michael C.
Brozovic, Marina
Benner, Lance A. M.
Giorgini, Jon D.
Magri, Christopher
TI Radar imaging and physical characterization of near-Earth Asteroid
(162421) 2000 ET70
SO ICARUS
LA English
DT Article
DE Near-Earth objects; Asteroids; Radar observations; Orbit determination
ID OPTICAL OBSERVATIONS; 1999 KW4; BINARY; POPULATION; IMAGES; MODEL;
EVOLUTION; GOLEVKA; ORIGIN; SHAPE
AB We observed near-Earth Asteroid (162421) 2000 ET70 using the Arecibo and Goldstone radar systems over a period of 12 days during its close approach to the Earth in February 2012. We obtained continuous wave spectra and range-Doppler images with range resolutions as fine as 15 m. Inversion of the radar images yields a detailed shape model with an effective spatial resolution of 100 m. The asteroid has overall dimensions of 2.6 km x 2.2 km x 2.1 km (5% uncertainties) and a surface rich with kilometer-scale ridges and concavities. This size, combined with absolute magnitude measurements, implies an extremely low albedo (similar to 2%). It is a principal axis rotator and spins in a retrograde manner with a sidereal spin period of 8.96 +/- 0.01 h. In terms of gravitational slopes evaluated at scales of 100 m, the surface seems mostly relaxed with over 99% of the surface having slopes less than 30 degrees, but there are some outcrops at the north pole that may have steeper slopes. Our precise measurements of the range and velocity of the asteroid, combined with optical astrometry, enables reliable trajectory predictions for this potentially hazardous asteroid in the interval 460-2813. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Naidu, Shantanu P.; Margot, Jean-Luc; Busch, Michael W.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Margot, Jean-Luc] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Taylor, Patrick A.; Nolan, Michael C.] Arecibo Observ, Arecibo, PR 00612 USA.
[Brozovic, Marina; Benner, Lance A. M.; Giorgini, Jon D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Magri, Christopher] Univ Maine, Farmington, ME 04938 USA.
RP Naidu, SP (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, 595 Charles Young Dr East,5656 Geol Bldg, Los Angeles, CA 90095 USA.
EM spn@ucla.edu
RI Nolan, Michael/H-4980-2012; Margot, Jean-Luc/A-6154-2012
OI Nolan, Michael/0000-0001-8316-0680; Margot, Jean-Luc/0000-0001-9798-1797
FU National Science Foundation (NSF) [AST-1100968]; Ana G.
Mendez-Universidad Metropolitana; Universities Space Research
Association; National Aeronautics and Space Administration (NASA); NASA
under the Science Mission Directorate Research and Analysis Programs;
NASA Near-Earth Object Observations Program [NNX12-AF24G]; NSF Astronomy
and Astrophysics Program [AST-1211581]
FX We thank the staff at Arecibo and Goldstone for assistance with the
observations. The Arecibo Observatory is operated by SRI International
under cooperative agreement AST-1100968 with the National Science
Foundation (NSF), and in alliance with Ana G. Mendez-Universidad
Metropolitana, and the Universities Space Research Association. Some of
this work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration (NASA). This material is based in part upon
work supported by NASA under the Science Mission Directorate Research
and Analysis Programs. The Arecibo Planetary Radar is supported in part
by NASA Near-Earth Object Observations Program NNX12-AF24G. S.P.N. and
J.L.M. were partially supported by NSF Astronomy and Astrophysics
Program AST-1211581.
NR 42
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 323
EP 335
DI 10.1016/j.icarus.2013.05.025
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200028
ER
PT J
AU Urata, RA
Toon, OB
AF Urata, Richard A.
Toon, Owen B.
TI A new general circulation model for Mars based on the NCAR Community
Atmosphere Model
SO ICARUS
LA English
DT Article
DE Mars; Mars, Atmosphere; Mars, Climate
ID THERMAL EMISSION SPECTROMETER; CONVECTIVE BOUNDARY-LAYER; MARTIAN POLAR
CAPS; CARBON-DIOXIDE; NUMERICAL-SIMULATION; VIKING OBSERVATIONS;
DIURNAL-VARIATIONS; SURFACE PRESSURE; WATER CYCLE; CO2
AB We introduce and present results from a new general circulation model for Mars adapted from the National Center for Atmospheric Research (NCAR) Community Atmosphere Model (CAM) version 3.1 terrestrial model. The radiative transfer has been replaced with a two-stream correlated-k scheme with carbon dioxide gas absorption coefficients suited for Mars. A time-invariant dust field is assumed with a Conrath (Conrath, B.J. [1975]. Icarus 24, 34-46) vertical distribution. Carbon dioxide is allowed to sublimate and condense at the surface, and the mass is removed from the atmosphere. The topography is averaged from MOLA data. The surface albedos and thermal inertias are derived from TES observations. The model is freely distributed to interested users.
Comparisons between model temperatures, and spacecraft and Lander observations show agreement within +/- 10 K, depending on dust concentration. The annual pressure cycle is typically within 20 Pa of Viking Lander observations, however the model underestimates the surface pressure during southern summer, possibly due to increased dust activity that is not reflected in the model. Predicted model boundary layer depths are typically within a few hundred meters of observations, and tend to depend inversely on surface pressure, agreeing with observations. Published by Elsevier Inc.
C1 [Urata, Richard A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Toon, Owen B.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Toon, Owen B.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
RP Urata, RA (reprint author), NASA, Ames Res Ctr, Bldg N245,Room 207, Moffett Field, CA 94035 USA.
EM richard.urata@colorado.edu
FU NASA [NNX08AV46H, NNX10AR17G]
FX We would like to acknowledge Dr. Timothy Michaels at the Southwest
Research Institute for providing the Fortran 90 radiative transfer code,
and the NASA Graduate Student Research Program for funding the research
(NNX08AV46H). Some support was also provided by the NASA Exobiology
Program (NNX10AR17G).
NR 66
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 336
EP 354
DI 10.1016/j.icarus.2013.05.017
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200029
ER
PT J
AU Ohtake, M
Pieters, CM
Isaacson, P
Besse, S
Yokota, Y
Matsunaga, T
Boardman, J
Yamomoto, S
Haruyama, J
Staid, M
Mall, U
Green, RO
AF Ohtake, M.
Pieters, C. M.
Isaacson, P.
Besse, S.
Yokota, Y.
Matsunaga, T.
Boardman, J.
Yamomoto, S.
Haruyama, J.
Staid, M.
Mall, U.
Green, R. O.
TI One Moon, Many Measurements 3: Spectral reflectance
SO ICARUS
LA English
DT Article
DE Moon; Mineralogy; Spectroscopy
ID NEAR-INFRARED SPECTROMETER; KAGUYA MULTIBAND IMAGER; MINERALOGY MAPPER
M-3; SELENE; CHANDRAYAAN-1; CALIBRATION; IRRADIANCE; SURFACE; CAMERA
AB Remote-sensing datasets obtained by each instrument aboard Selenological and Engineering Explorer (SELENE) and Chandrayaan-1 have not been compared directly, and the characteristics of each instrument's data, which may reflect the observation conditions of each instrument and/or residual error in instrument calibration, are unknown. This paper describes the basic characteristics of the data derived by each instrument, briefly describes the data-processing conversion from radiance to reflectance, and demonstrates what we can achieve by combining data obtained by different instruments on different missions (five remote-sensing instruments and an Earth-based telescope). The results clearly demonstrate that the spectral shapes of the instruments are comparable and thus enable us to estimate the composition of each geologic unit, although absolute reflectances differ slightly in some cases. (C) 2013 Published by Elsevier Inc.
C1 [Ohtake, M.; Haruyama, J.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Pieters, C. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Isaacson, P.] Univ Hawaii, Honolulu, HI 96822 USA.
[Besse, S.] ESA ESTEC, NL-2200 AG Noordwijk, Netherlands.
[Yokota, Y.; Matsunaga, T.; Yamomoto, S.] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan.
[Boardman, J.] Analyt Imaging & Geophys LLC, Boulder, CO 80303 USA.
[Staid, M.] Planetary Sci Inst, Tucson, AZ USA.
[Mall, U.] Max Planck Inst, Lindau, Germany.
[Green, R. O.] Jet Prop Lab, Pasadena, CA 91011 USA.
RP Ohtake, M (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
EM ohtake.makiko@jaxa.jp
OI Besse, Sebastien/0000-0002-1052-5439
FU NASA Lunar Science Institute [NNA09DB34A]
FX We are grateful for the dedication and accomplishments of the SELENE and
Chandrayaan-1 flight teams who successfully provided extensive new lunar
data to the science community. Participation by several authors in this
analysis was supported through the NASA Lunar Science Institute
(NNA09DB34A). This is SOEST publication number 8925 and HIGP publication
number 2012.
NR 37
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 364
EP 374
DI 10.1016/j.icarus.2013.05.010
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200031
ER
PT J
AU Janssen, MA
Ingersoll, AP
Allison, MD
Gulkis, S
Laraia, AL
Baines, KH
Edgington, SG
Anderson, YZ
Kelleher, K
Oyafuso, FA
AF Janssen, M. A.
Ingersoll, A. P.
Allison, M. D.
Gulkis, S.
Laraia, A. L.
Baines, K. H.
Edgington, S. G.
Anderson, Y. Z.
Kelleher, K.
Oyafuso, F. A.
TI Saturn's thermal emission at 2.2-cm wavelength as imaged by the Cassini
RADAR radiometer
SO ICARUS
LA English
DT Article
DE Saturn, Atmosphere; Atmospheres, Structure; Atmospheres, Composition;
Radiative transfer; Radio observations
ID TITANS SURFACE; LABORATORY MEASUREMENTS; JUPITERS ATMOSPHERE;
MICROWAVE-SPECTRUM; OUTER PLANETS; TEMPERATURES; ABSORPTION; AMMONIA;
PROBE; RING
AB We present well-calibrated, high-resolution maps of Saturn's thermal emission at 2.2-cm wavelength obtained by the Cassini RADAR radiometer through the Prime and Equinox Cassini missions, a period covering approximately 6 years. The absolute brightness temperature calibration of 2% achieved is more than twice better than for all previous microwave observations reported for Saturn, and the spatial resolution and sensitivity achieved each represent nearly an order of magnitude improvement. The brightness temperature of Saturn in the microwave region depends on the distribution of ammonia, which our radiative transfer modeling shows is the only significant source of absorption in Saturn's atmosphere at 2.2-cm wavelength. At this wavelength the thermal emission comes from just below and within the ammonia cloud-forming region, and yields information about atmospheric circulations and ammonia cloud-forming processes. The maps are presented as residuals compared to a fully saturated model atmosphere in hydrostatic equilibrium. Bright regions in these maps are readily interpreted as due to depletion of ammonia vapor in, and, for very bright regions, below the ammonia saturation region. Features seen include the following: a narrow equatorial band near full saturation surrounded by bands out to about 10 degrees planetographic latitude that demonstrate highly variable ammonia depletion in longitude; narrow bands of depletion at -35 degrees latitude; occasional large oval features with depleted ammonia around -45 degrees latitude; and the 2010-2011 storm, with extensive saturated and depleted areas as it stretched halfway around the planet in the northern hemisphere. Comparison of the maps over time indicates a high degree of stability outside a few latitudes that contain active regions. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Janssen, M. A.; Gulkis, S.; Baines, K. H.; Edgington, S. G.; Anderson, Y. Z.; Kelleher, K.; Oyafuso, F. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ingersoll, A. P.; Laraia, A. L.] CALTECH, Pasadena, CA 91125 USA.
[Allison, M. D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Janssen, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM michael.a.janssen@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA); NASA through the
Cassini Data Analysis and Participating Scientist (CDAPS) Program
[10-CDAP10-0051]; Cassini RADAR team
FX This research was conducted at the Jet Propulsion Laboratory (JPL),
California Institute of Technology, under contract with the National
Aeronautics and Space Administration (NASA). It is partly based upon
work supported by NASA under Grant No. 10-CDAP10-0051 issued through the
Cassini Data Analysis and Participating Scientist (CDAPS) Program. We
acknowledge Sushil Atreya, Lena Adams, and Virgil Adumantroi for their
invaluable contributions to the Juno Atmospheric Microwave Radiative
Transfer (JAMRT) program, P. Steffes for discussions on the microwave
absorption of ammonia in the Saturn atmosphere, Scott Bolton, Steve
Levin, and the Juno project for their encouragement of this work, Alice
Le Gall for her contributions to the calibration, Bryan Butler for
discussion of the capabilities of ground-based interferometers, and
Glenn Orton for useful discussions on sources of microwave absorption as
well as related visual and infrared observations of giant planet
atmospheres. We also gratefully acknowledge the Cassini RADAR team in
general for their support, along with those who designed, developed and
operate the Cassini/Huygens mission, which is a joint endeavor of NASA,
the European Space Agency (ESA), and the Italian Space Agency (ASI) and
is managed by JPL/Caltech under a contract with NASA.
NR 47
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U1 1
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
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 522
EP 535
DI 10.1016/j.icarus.2013.06.008
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200043
ER
PT J
AU Deau, E
Dones, L
Charnoz, S
West, RA
Brahic, A
Decriem, J
Porco, CC
AF Deau, Estelle
Dones, Luke
Charnoz, Sebastien
West, Robert A.
Brahic, Andre
Decriem, Judicael
Porco, Carolyn C.
TI The opposition effect in Saturn's main rings as seen by Cassini ISS: 1.
Morphology of phase functions and dependence on the local optical depth
SO ICARUS
LA English
DT Article
DE Planetary rings; Saturn, Rings; Photometry
ID SOLAR-SYSTEM OBJECTS; WEAK-LOCALIZATION; HST OBSERVATIONS;
LIGHT-SCATTERING; PHOTOMETRY; CURVES; MEDIA; SIMULATIONS; POLARIMETRY;
MECHANISMS
AB During the Prime mission (2004-2008), the Cassini cameras captured the opposition effect in Saturn's main rings with a fine radial resolution at extremely small phase angles. Phase functions were extracted for 211 different radial locations in the main ring system (135 in the broadband clear filter of the Wide Angle Camera at 635 nm, 76 in four narrowband color filters (at the respective central wavelengths 440, 568, 650, and 752 nm for the Narrow Angle Camera and 460, 567, 649, and 742 nm for the Wide Angle Camera). The morphology of the observed opposition surges is fitted with a simple linear model in order to derive three useful parameters - the amplitude A, the width of the surge HWHM, and the slope S at larger phase angles - throughout the whole main ring system. In agreement with previous studies, the opposition surge is found to vary substantially across the ring system: whereas values of A and HWHM are nearly constant across the A and B Rings, they show strong local variations for the C Ring and the Cassini Division. Thanks to the high spatial resolution of Cassini images, the opposition surges are obtained for very narrow regions, allowing us to study the effect of the local normal optical depth (tau) on the surge. For tau>0.7, A(tau) and HWHM(tau) are nearly constant (1.3 degrees and 0.25 degrees, respectively) across the whole ring system. For tau<0.7, A(tau) and HWHM(tau) exhibit clear decreasing trends for the A, B and C Rings only. Conversely, points from the Cassini Division show a very large dispersion in both A and HWHM, with no visible trend. The slope S is found to be an increasing function of the optical depth across the full ring system. A trend S proportional to tau(0.5) is observed, in qualitative agreement with a geometrical description of the shadow hiding effect. No strong trend of A, HWHM and S with the wavelength of observation was found. We also tabulate the fit parameters for the opposition surge of 139 regions in the clear filter for future comparison with numerical simulations and photometric models. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Deau, Estelle; West, Robert A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Deau, Estelle; Decriem, Judicael] CEA Saclay, Serv Astrophys, Lab AIM, F-91191 Gif Sur Yvette, France.
[Dones, Luke] SW Res Inst, Boulder, CO 80302 USA.
[Charnoz, Sebastien; Brahic, Andre] Univ Paris 07, Lab AIM, F-75205 Paris 13, France.
[Porco, Carolyn C.] CICLOPS, Space Sci Inst, Boulder, CO 80301 USA.
RP Deau, E (reprint author), NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Estelle.Deau@jpl.nasa.gov
FU French Conseil Regional de la Martinique; NASA Postdoctoral Program led
by OakRidge Associated Universities (ORAU); Cassini project
FX This work was supported by the French Conseil Regional de la Martinique,
the NASA Postdoctoral Program led by OakRidge Associated Universities
(ORAU), and the Cassini project.
NR 65
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 591
EP 603
DI 10.1016/j.icarus.2013.01.015
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200048
ER
PT J
AU Nolan, MC
Magri, C
Howell, ES
Benner, LAM
Giorgini, JD
Hergenrother, CW
Hudson, RS
Lauretta, DS
Margot, JL
Ostro, SJ
Scheeres, DI
AF Nolan, Michael C.
Magri, Christopher
Howell, Ellen S.
Benner, Lance A. M.
Giorgini, Jon D.
Hergenrother, Carl W.
Hudson, R. Scott
Lauretta, Dante S.
Margot, Jean-Luc
Ostro, Steven J.
Scheeres, Daniel I.
TI Shape model and surface properties of the OSIRIS-REx target Asteroid
(101955) Bennu from radar and lightcurve observations
SO ICARUS
LA English
DT Article
DE Radar observations; Asteroids, Surfaces; Asteroids, Rotation; Asteroid
Bennu
ID 433 EROS; ARECIBO; ITOKAWA; OBJECTS
AB We determine the three-dimensional shape of near-Earth Asteroid (101955) Bennu based on radar images and optical lightcurves. Bennu was observed both in 1999 at its discovery apparition, and in 2005 using the 12.6-cm radar at the Arecibo Observatory and the 3.5-cm radar at the Goldstone tracking station. Data obtained in both apparitions were used to construct a shape model of this object. Observations were also obtained at many other wavelengths to characterize this object, some of which were used to further constrain the shape modeling. The lightcurve data, along with an initial determination of the rotation period derived from them, simplified and improved the shape modeling.
Below we briefly describe the observations and shape modeling process. We discuss the shape model and the implications for the possible formation and evolution of this object. We also describe the importance and limitations of the shape model in view of the fact that this object is the target of the OSIRIS-REx spacecraft mission. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Nolan, Michael C.; Howell, Ellen S.] Arecibo Observ, Arecibo, PR 00612 USA.
[Magri, Christopher] Univ Maine, Farmington, ME 04938 USA.
[Benner, Lance A. M.; Giorgini, Jon D.; Ostro, Steven J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hergenrother, Carl W.; Lauretta, Dante S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Hudson, R. Scott] Washington State Univ, Richland, WA 99354 USA.
[Margot, Jean-Luc] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90295 USA.
[Scheeres, Daniel I.] Univ Colorado, Boulder, CO 80309 USA.
RP Nolan, MC (reprint author), Arecibo Observ, HC 3 Box 53995, Arecibo, PR 00612 USA.
EM nolan@naic.edu
RI Nolan, Michael/H-4980-2012; Margot, Jean-Luc/A-6154-2012
OI Nolan, Michael/0000-0001-8316-0680; Margot, Jean-Luc/0000-0001-9798-1797
FU OSIRIS-REx project [NNM10AA11C]; NSF [AST-0205975]; National Aeronautics
and Space Administration (NASA); NASA; [NNX10AP64G]; [NNX12AF24G]
FX We thank Yu. Krugly for providing the original lightcurve data from 1999
for modeling. The Arecibo Observatory is part of the National Astronomy
and Ionosphere Center, which at the time of observation was operated by
Cornell University for the National Science Foundation. MCN and ESH were
supported by NNX10AP64G, NNX12AF24G and funding from the OSIRIS-REx
project, NNM10AA11C. CM was partially supported by NSF Grant
AST-0205975. Some of this work was performed at the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under contract
with the National Aeronautics and Space Administration (NASA). This
material is based in part upon work supported by NASA under the Science
Mission Directorate Research and Analysis Programs.
NR 36
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U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 629
EP 640
DI 10.1016/j.icarus.2013.05.028
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200051
ER
PT J
AU Laraia, AL
Ingersoll, AP
Janssen, MA
Gulkis, S
Oyafuso, F
Allison, M
AF Laraia, A. L.
Ingersoll, A. P.
Janssen, M. A.
Gulkis, S.
Oyafuso, F.
Allison, M.
TI Analysis of Saturn's thermal emission at 2.2-cm wavelength: Spatial
distribution of ammonia vapor
SO ICARUS
LA English
DT Article
DE Saturn, Atmosphere; Atmospheres, Structure; Atmospheres, Composition;
Atmospheres, Dynamics; Radio observations
ID JUPITERS ATMOSPHERE; MOIST CONVECTION; CASSINI ISS; JOVIAN THUNDERCLOUD;
RADIO OBSERVATIONS; GIANT PLANETS; IMAGES; STORM; DYNAMICS; MODEL
AB This work focuses on determining the latitudinal structure of ammonia vapor in Saturn's cloud layer near 1.5 bars using the brightness temperature maps derived from the Cassini RADAR (Elachi et al. [2004], Space Sci. Rev. 115, 71-110) instrument, which works in a passive mode to measure thermal emission from Saturn at 2.2-cm wavelength. We perform an analysis of five brightness temperature maps that span epochs from 2005 to 2011, which are presented in a companion paper by Janssen et al. (Janssen, M.A., Ingersoll, A.P., Allison, M.D., Gulkis, S., Laraia, A.L., Baines, K., Edgington, S., Anderson, Y., Kelleher, K., Oyafuso, F. [2013]. Icarus, this issue). The brightness temperature maps are representative of the spatial distribution of ammonia vapor, since ammonia gas is the only effective opacity source in Saturn's atmosphere at 2.2-cm wavelength. Relatively high brightness temperatures indicate relatively low ammonia relative humidity (RH), and vice versa. We compare the observed brightness temperatures to brightness temperatures computed using the Juno atmospheric microwave radiative transfer (JAMRT) program which includes both the means to calculate a tropospheric atmosphere model for Saturn and the means to carry out radiative transfer calculations at microwave frequencies. The reference atmosphere to which we compare has a 3x solar deep mixing ratio of ammonia (we use 1.352 x 10(-4) for the solar mixing ratio of ammonia vapor relative to H-2; see Atreya [2010]. In: Galileo's Medicean Moons - Their Impact on 400 years of Discovery. Cambridge University Press, pp. 130-140 (Chapter 16)) and is fully saturated above its cloud base. The maps are comprised of residual brightness temperatures-observed brightness temperature minus the model brightness temperature of the saturated atmosphere.
The most prominent feature throughout all five maps is the high brightness temperature of Saturn's subtropical latitudes near +/- 9 degrees (planetographic). These latitudes bracket the equator, which has some of the lowest brightness temperatures observed on the planet. The observed high brightness temperatures indicate that the atmosphere is sub-saturated, locally, with respect to fully saturated ammonia in the cloud region. Saturn's northern hemisphere storm was also captured in the March 20, 2011 map, and is very bright, reaching brightness temperatures of 166 K compared to 148 K for the saturated atmosphere model. We find that both the subtropical bands and the 2010-2011 northern storm require very low ammonia RH below the ammonia cloud layer, which is located near 1.5 bars in the reference atmosphere, in order to achieve the high brightness temperatures observed. The disturbances in the southern hemisphere between -42 degrees and -47 degrees also require very low ammonia RH at levels below the ammonia cloud base. Aside from these local and regional anomalies, we find that Saturn's atmosphere has on average 70 +/- 15% ammonia relative humidity in the cloud region. We present three options to explain the high 2.2-cm brightness temperatures. One is that the dryness, i.e., the low RH, is due to higher than average atmospheric temperatures with constant ammonia mixing ratios. The second is that the bright subtropical bands represent dry zones created by a meridionally overturning circulation, much like the Hadley circulation on Earth. The last is that the drying in both the southern hemisphere storms and 2010-2011 northern storm is an intrinsic property of convection in giant planet atmospheres. Some combination of the latter two options is argued as the likely explanation. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Laraia, A. L.; Ingersoll, A. P.] CALTECH, Pasadena, CA 91125 USA.
[Janssen, M. A.; Gulkis, S.; Oyafuso, F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Allison, M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Laraia, AL (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM alaraia@caltech.edu
FU National Aeronautics and Space Administration (NASA) [10-CDAP10-0051];
National Science Foundation (NSF)
FX This research was conducted at the California Institute of Technology
under contract with the National Aeronautics and Space Administration
(NASA). It is partly based upon work supported by NASA under Grant No.
10-CDAP10-0051 issued through the Cassini Data Analysis and
Participating Scientist (CDAPS) Program. A. Laraia was partially funded
by a National Science Foundation (NSF) Graduate Research Fellowship
Program (GRFP) fellowship. We acknowledge Sushil Atreya, Lena Adams, and
Virgil Adumantroi for their invaluable contributions to the Juno
atmospheric microwave radiative transfer (JAMRT) program. We would also
like to acknowledge Kevin Baines for useful discussions on comparing
RADAR and VIMS data.
NR 43
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U1 3
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
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 641
EP 654
DI 10.1016/j.icarus.2013.06.017
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200052
ER
PT J
AU Pankine, AA
Tamppari, LK
Bandfield, JL
McConnochie, TH
Smith, MD
AF Pankine, Alexey A.
Tamppari, Leslie K.
Bandfield, Joshua L.
McConnochie, Timothy H.
Smith, Michael D.
TI Retrievals of martian atmospheric opacities from MGS TES nighttime data
SO ICARUS
LA English
DT Article
DE Mars, Atmosphere; Atmospheres, Structure; Infrared observations
ID THERMAL EMISSION SPECTROMETER; WATER-ICE CLOUDS; GENERAL-CIRCULATION
MODEL; INTERANNUAL VARIABILITY; MARS; CYCLE; TEMPERATURES; EVOLUTION;
CLIMATE; VAPOR
AB We describe a new retrieval algorithm that accounts for the presence of the systematic background radiance error in the infrared spectra collected by the Mars Global Surveyor (MGS) Thermal Emission Spectrometer (TES). The algorithm is used to retrieve dust and water ice cloud opacities from the nighttime TES nadir spectra. Nighttime dust opacities are systematically higher than the day opacities by similar to 30%, which is attributed to uncertainties of the retrieval model. Nighttime water ice cloud opacities could be systematically underestimated by a factor of similar to 2, depending on the ice particle size. Uncertainty of the ice particle sizes does not affect clouds spatial distributions. Independent of the ice particle sizes, the night clouds have higher opacity and are more extensive than the day clouds. Spatial and seasonal variability of nighttime ice clouds is investigated over a time span of 2.5 Mars years of TES observations. Seasonal evolution of the nighttime clouds is similar to the evolution of daytime clouds, with the maximum areal extent and highest opacities reached during the aphelion season (northern spring and summer) in the equatorial belt. A secondary increase in the ice cloud opacities is observed during perihelion season (southern spring and summer). During southern summer extensive clouds are found over and around the Tharsis volcanoes, Olympus Mons, western Valles Marineris, and between Syrtis Major and Elysium Planitia. This pattern of diurnal spatial variability is consistent with the strong influence of thermal tides on cloud formation. Perihelion season is characterized by the thinner nighttime clouds appearing south of the Tharsis and western Valles Marineris and north of the Hellas basin. The seasonal spatial patterns of the nighttime water ice clouds are highly repeatable year over year. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Pankine, Alexey A.] Space Sci Inst, Boulder, CO 80301 USA.
[Tamppari, Leslie K.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Bandfield, Joshua L.] Univ Washington, Seattle, WA 98195 USA.
[McConnochie, Timothy H.] Univ Maryland, College Pk, MD 20742 USA.
[Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Pankine, AA (reprint author), Space Sci Inst, Boulder, CO 80301 USA.
EM apankine@spacescience.org
FU Mars Data Analysis program
FX We thank two anonymous reviewers for their comments. This research was
carried out at the Space Science Institute and Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration and funded through the
Mars Data Analysis program.
NR 48
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U1 0
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
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 708
EP 722
DI 10.1016/j.icarus.2013.06.024
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200058
ER
PT J
AU Reach, WT
Kelley, MS
Vaubaillon, J
AF Reach, William T.
Kelley, Michael S.
Vaubaillon, Jeremie
TI Survey of cometary CO2, CO, and particulate emissions using the Spitzer
Space Telescope
SO ICARUS
LA English
DT Article
DE Comets; Comets, Coma; Infrared observations
ID O1 HALE-BOPP; OH LINE-SHAPES; EXPANSION VELOCITY; PERIOD COMETS; LIGHT
CURVES; HARTLEY 2; NUCLEI; DUST; GAS; ATMOSPHERES
AB We surveyed 23 comets using the Infrared Array Camera on the Spitzer Space Telescope in wide filters centered at 3.6 and 4.5 mu m. Emission in the 3.6 mu m filter arises from sunlight scattered by dust grains; the 3.6 gm images generally have a coma near the nucleus and a tail in the antisolar direction due to dust grains swept back by solar radiation pressure. The 4.5 mu m filter contains scattered sunlight by, and thermal emission from, the same dust grains, as well as strong emission lines from CO2 and CO gas. The 4.5 mu m images are often much brighter than could be explained by dust grains, and they show sometimes distinct morphologies, in which cases we infer they are dominated by gas. Based on the ratio of 4.5-3.6 mu m brightness, we classify the survey comets as CO2 + CO 'rich' and 'poor'. This classification is correlated with previous classifications by A'Hearn based on carbon-chain molecule abundance, in the sense that comets classified as 'depleted' in carbon-chain molecules are also 'poor' in CO2 + CO. The gas emission in the IRAC 4.5 mu m images is characterized by a smooth morphology, typically a fan in the sunward hemisphere with a radial profile that varies approximately as the inverse of projected distance from the nucleus, as would apply for constant production and free expansion. There are very significant radial and azimuthal enhancements in many of the comets, and these are often distinct between the gas and dust, indicating that ejection of solid material may be driven either by H2O or CO2. Notable features in the images include the following. There is a prominent loop of gas emission from 103P/Hartley 2, offset toward the sunward direction; the loop could be due to an outburst of CO2 before the Spitzer image. Prominent, double jets are present in the image of 88P/Howell, with one directed nearly toward the Sun and the other closer to the terminator (but still on the daytime hemisphere). A prominent single jet is evident for C/2002 T7 (LINEAR), 22P/Kopff and 81P/Wild 2. Spirals are apparent in 29P/Schwassmann-Wachmann 1 and C/2006 W3 (Christensen); we measure a rotation rate of 21 h for the latter comet. Arcs (possibly parts of a spiral) are apparent in the images of 10P/Tempel 2, and 2P/Encke. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Reach, William T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kelley, Michael S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Vaubaillon, Jeremie] Inst Mecan Celeste & Calcul Ephemerides, F-75014 Paris, France.
RP Reach, WT (reprint author), Univ Space Res Assoc, Stratospher Observ Infrared Astron, NASA, Ames Res Ctr, MS 232-12, Moffett Field, CA 94035 USA.
EM wreach@sofia.usra.edu
OI Kelley, Michael/0000-0002-6702-7676; Reach, William/0000-0001-8362-4094
FU NASA through JPL/Caltech
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. Support
for this work was provided by NASA through an award issued by
JPL/Caltech.
NR 48
TC 20
Z9 20
U1 1
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
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 777
EP 797
DI 10.1016/j.icarus.2013.06.011
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200062
ER
PT J
AU Michalski, JR
Niles, PB
Cuadros, J
Baldridge, AM
AF Michalski, Joseph R.
Niles, P. B.
Cuadros, J.
Baldridge, A. M.
TI Multiple working hypotheses for the formation of compositional
stratigraphy on Mars: Insights from the Mawrth Vallis region
SO ICARUS
LA English
DT Article
DE Mars; Infrared observations; Mineralogy; Geological processes
ID INTERIOR LAYERED DEPOSITS; MERIDIANI-PLANUM; OMEGA/MARS EXPRESS; THERMAL
INERTIA; CLAY-MINERALS; ARABIA TERRA; ORIGIN; POLAR; WATER; CLIMATE
AB A unique aspect of martian geology is the presence of similar compositional stratigraphy observed in many locations throughout the surface. Where the Al-rich and Fe/Mg-rich clay minerals occur together, aluminous clays typically overly layered ferromagnesian clays, possibly indicating that precipitation-driven leaching occurred in a warmer, wetter climate. Sulfates generally occurring stratigraphically above clays could be relics of a global environmental shift between clay-forming and sulfate forming epochs. These compositional relationships speak to an important aspect of the martian geosystem that is yet poorly understood. We synthesized recent ideas to produce several working hypotheses for the formation of compositional stratigraphy on Mars and tested the hypotheses on well-exposed sulfate- and clay-bearing rocks found in the Mawrth Vallis region. In the Mawrth Vallis area, interpretations of compositional stratigraphy are strongly constrained by the fact that the sulfates and clays occur within a friable unit (probably loessite or tephra) that was deposited unconformably onto cratered terrain of fundamentally different character. Within the friable unit, the presence of aluminous- clays over ferromagnesian clays might represent evidence for leaching associated with rainfall, but the presence of montmorillonite, beidellite, and sulfates argue against intense leaching as a dominant process. We suggest that ice/snow-mediated chemical weathering of dust could produce a deposit consistent with the observations through hydrolysis reactions facilitated by acidic, briny solutions within the icy dust deposit. Slow downward transport of Mg2+ and possibly Fe2+ in these solutions could potentially have produced the crude compositional stratigraphy, but regional scale leaching of basaltic bedrock by rainfall is unlikely to explain the observations. Because both clays and sulfates are found within draping, friable sedimentary deposits that occur at a range of elevations, formation of the alteration minerals by upwelling groundwater is implausible. The locations where compositional stratigraphy is observed may not be relics of a global environmental change, but rather they cold represent the locations where significant deposits of snow/ice and dust/ash once existed. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Michalski, Joseph R.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Michalski, Joseph R.; Cuadros, J.] Nat Hist Museum, Dept Earth Sci, London SW7 5BD, England.
[Niles, P. B.] NASA Johnson Space Ctr, Richardson, TX 75080 USA.
[Baldridge, A. M.] St Marys Coll Calif, Moraga, CA 94556 USA.
RP Michalski, JR (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
EM michalski@psi.edu; paul.b.niles@nasa.gov; j.caudros@nhm.ac.uk;
amb19@stmarys-ca.edu
NR 94
TC 15
Z9 15
U1 1
U2 14
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 SEP-OCT
PY 2013
VL 226
IS 1
BP 816
EP 840
DI 10.1016/j.icarus.2013.05.024
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200064
ER
PT J
AU Rhoden, AR
Hurford, TA
AF Rhoden, Alyssa Rose
Hurford, Terry A.
TI Lineament azimuths on Europa: Implications for obliquity and
non-synchronous rotation
SO ICARUS
LA English
DT Article
DE Europa; Tectonics; Rotational dynamics
ID STRIKE-SLIP DISPLACEMENT; TIDAL STRESSES; GALILEAN SATELLITES; GROWTH
MECHANICS; CRACK AZIMUTHS; ICE SHELLS; PATTERNS; CONSTRAINTS; SEQUENCE;
FRACTURE
AB Lineaments are thought to form as tensile cracks due to tidal stress, which is driven mainly by Europa's eccentric orbit. However, this model would not produce the wide range of lineament azimuths observed on Europa unless the stress in a given region, or the conditions for fault failure, change over time. In this work, we test the ability of two mechanisms that would alter the stress field over time to account for the observed lineament azimuths: non-synchronous rotation and spin pole precession. First, we revisit previous analysis of lineaments and find that an underlying assumption used to predict their azimuths was inconsistently applied. After revising these predictions, we incorporate the effects of a non-zero obliquity, which has been shown to influence the formation of other tidal-tectonic features. We then expand our analysis to include the effects of the time-variable phenomena, spin pole precession and non-synchronous rotation of the ice shell. We also consider additional failure assumptions to those used in previous work on lineament azimuths. We test our models against the azimuths of observed lineaments in the Bright Plains region of Europa. Without obliquity, we find that non-synchronous rotation is insufficient to explain the wide range of azimuths observed in this region. In the presence of obliquity, we find that either spin pole precession or non-synchronous rotation could produce wide variations in lineament azimuths. However, neither model can independently account for the observed distribution of azimuths in the Bright Plains region. In fact, a model in which all of the lineaments are assumed to form at random orientations outperforms the non-synchronous rotation model in our statistical tests. The model with the highest likelihood of producing the observations is one in which 45% of the lineaments formed as predicted in the precession model, 55% formed at random orientations, and older lineaments are less represented in the tectonic record. Given the relative timescales expected for spin pole precession and non-synchronous rotation, it makes sense that the signal of precession is more apparent in the tectonic record. These results are in good agreement with assessments of strike-slip faults; modeling of both types of features indicates a large obliquity, the same spin pole direction during the most recent epoch of tectonic activity, a similar percentage of features that are not well-explained by the tidal model, and little evidence of non-synchronous rotation. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Rhoden, Alyssa Rose; Hurford, Terry A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rhoden, AR (reprint author), NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA.
EM Alyssa.R.Rhoden@nasa.gov
RI Hurford, Terry/F-2625-2012
FU NASA
FX The authors wish to thank P. Geissler and G. Collins for their
constructive reviews and E. Huff for assisting with the statistical
analysis. Funding for A. Rhoden was provided through the NASA
Postdoctoral Program.
NR 36
TC 5
Z9 5
U1 0
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 841
EP 859
DI 10.1016/j.icarus.2013.06.029
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200065
ER
PT J
AU Loeffler, MJ
Fama, M
Baragiola, RA
Carlson, RW
AF Loeffler, M. J.
Fama, M.
Baragiola, R. A.
Carlson, R. W.
TI Photolysis of H2O-H2O2 mixtures: The destruction of H2O2
SO ICARUS
LA English
DT Article
DE Europa; Ices, IR spectroscopy; Jupiter, satellites; Saturn, satellites;
Photochemistry
ID HYDROGEN-PEROXIDE; WATER ICE; GALILEAN SATELLITES; INFRARED-SPECTRA; ION
IRRADIATION; QUANTUM YIELDS; 193 NM; EUROPA; ULTRAVIOLET; ENCELADUS
AB We present laboratory results on the loss of H2O2 in solid H2O + H2O2 mixtures at temperatures between 21 and 145 K initiated by UV photolysis (193 nm). Using infrared spectroscopy and microbalance gravimetry, we measured the decrease of the 3.5 mu m infrared absorption band during UV irradiation and obtained a photodestruction cross section that varies with temperature, being lowest at 70 K. We use our results, along with our previously measured H2O2 production rates via ionizing radiation and ion energy fluxes from the spacecraft to compare H2O2 creation and destruction at icy satellites by ions from their planetary magnetosphere and from solar UV photons. We conclude that, in many cases, H2O2 is not observed on icy satellite surfaces because the H2O2 photodestruction rate is much higher than the production rate via energetic particles, effectively keeping the H2O2 infrared signature at or below the noise level. Published by Elsevier Inc.
C1 [Loeffler, M. J.] NASA, GSFC, Astrochem Lab, Greenbelt, MD 20771 USA.
[Loeffler, M. J.; Fama, M.; Baragiola, R. A.] Univ Virginia, Lab Atom & Surface Phys, Charlottesville, VA 22904 USA.
[Carlson, R. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Loeffler, MJ (reprint author), NASA, GSFC, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA.
EM mark.loeffler@nasa.gov
RI Loeffler, Mark/C-9477-2012;
OI Fama, Marcelo/0000-0003-3476-4669
FU NASA
FX This work is being funded by NASA Outer Solar System Program. M.
Loeffler thanks J. Cooper and P. Gerakines for useful discussions.
NR 61
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U1 1
U2 28
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 945
EP 950
DI 10.1016/j.icarus.2013.06.030
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200073
ER
PT J
AU Pieters, CM
Boardman, JW
Ohtake, M
Matsunaga, T
Haruyama, J
Green, RO
Mall, U
Staid, MI
Isaacson, PJ
Yokota, Y
Yamamoto, S
Besse, S
Sunshine, JM
AF Pieters, C. M.
Boardman, J. W.
Ohtake, M.
Matsunaga, T.
Haruyama, J.
Green, R. O.
Mall, U.
Staid, M. I.
Isaacson, P. J.
Yokota, Y.
Yamamoto, S.
Besse, S.
Sunshine, J. M.
TI One Moon, many measurements 1: Radiance values
SO ICARUS
LA English
DT Article
DE Moon; Regoliths; Spectroscopy
ID NEAR-INFRARED SPECTROMETER; KAGUYA MULTIBAND IMAGER; MINERALOGY MAPPER
M-3; SPECTRAL IRRADIANCE; SELENE; SURFACE; CHANDRAYAAN-1; CALIBRATION;
REFLECTANCE; CAMERA
AB Several modern optical instruments orbited the Moon during 2008 and 2009 onboard the SELENE and Chandrayaan-1 spacecraft and provided a welcomed feast of spectroscopic data to be used for scientific analyses. The different spatial and spectral resolutions of these sensors along with diverse illumination geometry during data acquisition make each set of data unique, and each instrument contributes special value to integrated science analyses. In order to provide the maximum science benefit, we have undertaken a careful cross-validation of radiance data among these orbital instruments and also a set of systematic data acquired using Earth-based telescopes. Most radiance values at 750 nm fall between 0 and 100 W/(m(2) mu m sr), but a small important fraction can be up to x2 to x3 that value, with the largest values occurring at the highest spatial resolution. All instruments are in agreement about overall spectral properties of lunar materials, but small systematic differences are documented between instruments. Lunar radiance values measured with remote sensors for landing sites are all not as high as that estimated from laboratory measurements of returned soil. This is largely because laboratory measurements of lunar soils cannot retain or duplicate the fine structure of lunar regolith found in the natural space environment. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Pieters, C. M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Boardman, J. W.] Analyt Imaging & Geophys LLC, Boulder, CO 80303 USA.
[Ohtake, M.; Haruyama, J.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Matsunaga, T.; Isaacson, P. J.; Yokota, Y.] Natl Inst Environm Studies, Ctr Environm Measurement & Anal, Tsukuba, Ibaraki 3058506, Japan.
[Green, R. O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mall, U.] Max Planck Inst Sonnensyst Forsch, Katlenburg Lindau, Germany.
[Staid, M. I.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Isaacson, P. J.] Univ Hawaii, Honolulu, HI 96822 USA.
[Besse, S.; Sunshine, J. M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Besse, S.] Estec, ESA, NL-2200 AG Noordwijk, Netherlands.
RP Pieters, CM (reprint author), Brown Univ, Dept Geol Sci, 324 Brook St, Providence, RI 02912 USA.
EM Carle_Pieters@brown.edu
OI Besse, Sebastien/0000-0002-1052-5439
FU NASA [NNM05AB26C]; NASA Lunar Science Institute [NNA09DB34A]
FX We are grateful for the dedication and accomplishments of the SELENE and
Chandrayaan-1 flight teams who successfully provided extensive new lunar
data to the science community. Initial M3 team participation
in these science analyses was supported by contract to Brown University
through the NASA Discovery Program (NNM05AB26C). The more detailed
integrated analyses were supported through the NASA Lunar Science
Institute (NNA09DB34A). This is SOEST Publication No. 2010 and HIGP
Publication No. 8923".
NR 43
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U1 0
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
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 951
EP 963
DI 10.1016/j.icarus.2013.07.008
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200074
ER
PT J
AU Zimmerman, MI
Farrell, WM
Stubbs, TJ
AF Zimmerman, M. I.
Farrell, W. M.
Stubbs, T. J.
TI Recursive plasma wake formation on the Moon and its effect on polar
volatiles
SO ICARUS
LA English
DT Article
DE Solar wind; Moon, surface; Ices
ID LUNAR POLES; SOLAR-WIND; EXPANSION; VACUUM; WATER; SPACECRAFT; HYDROXYL;
SURFACE; PLUME
AB Solar wind plasma flows almost horizontally in near-terminator regions of the Moon. One question is how does this plasma flow around topographic features like near-terminator mountains and polar craters? We present kinetic simulations of plasma inflow into a complicated polar crater having a second "child" crater within the "parent" crater (i.e., a 'crater-in-a-crater' model). We find that the effect on the inflowing ions of this second 'child' feature is a function of its position downstream relative to the primary crater wall: close to the wall where the solar wind is occulted there is little ion inflow and thus not a significant perturbation from the child obstruction. However, beyond about two crater wall heights downstream, there is substantial ion flow and the child obstruction will create a second ambipolar wake region similar to that created by the first obstruction. We also present a general analytical formalism that explains the most critical properties of the inflow perturbations. Finally, we consider the effect of the ion inflow into polar craters with 1% water 'frost' mixed within the top micron layers of the regolith. We find that in order to maintain equilibrium, a persistent frost most likely has to be maintained by a dynamic water source of similar to 10(9) molecules m(-2)s(-1) in polar craters to offset solar wind ion inflow sputtering losses. (C) 2013 The Authors. Published by Elsevier Inc. All rights reserved.
C1 [Zimmerman, M. I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NASA Lunar Sci Inst, Moffett Field, CA 94035 USA.
RP Zimmerman, MI (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM michael.i.zimmerman@nasa.gov
RI Farrell, William/I-4865-2013; Stubbs, Timothy/I-5139-2013
OI Stubbs, Timothy/0000-0002-5524-645X
FU NASA; LPROPS [NNX08AN76G]; NASA Lunar Science Institute; DREAM virtual
institute [NNX09AG78A]
FX 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 support of
LPROPS Grant NNX08AN76G and the NASA Lunar Science Institute and DREAM
virtual institute through Grant NNX09AG78A are gratefully acknowledged.
We gratefully acknowledge the generous allocation of computing resources
by Dr. Timothy McClanahan at NASA Goddard Space Flight Center.
NR 32
TC 5
Z9 5
U1 1
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
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 992
EP 998
DI 10.1016/j.icarus.2013.06.013
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200078
ER
PT J
AU Keihm, S
Kamp, L
Gulkis, S
Hofstadter, M
Lee, S
Janssen, M
Choukroun, M
AF Keihm, Stephen
Kamp, Lucas
Gulkis, Samuel
Hofstadter, Mark
Lee, Seungwon
Janssen, Michael
Choukroun, Mathieu
TI Reconciling main belt asteroid spectral flux density measurements with a
self-consistent thermophysical model
SO ICARUS
LA English
DT Article
DE Asteroids, Surfaces; Asteroids, Composition; Regoliths; Infrared
observations; Radio observations
ID HUBBLE-SPACE-TELESCOPE; ROSETTA FLY-BY; 21 LUTETIA; THERMAL PHYSICS;
SUBMILLIMETER OBSERVATIONS; PLANETARY SURFACES; RADIOMETRIC METHOD;
PHOTOMETRIC DATA; LUNAR-SURFACE; VESTA
AB Thermophysical models consistent with Earth's Moon and infrared and submillimeter measurements obtained during the Rosetta fly-by of Asteroid (21) Lutetia have been applied to computations of thermal fluxes from Asteroids (4) Vesta, (1) Ceres, (2) Pallas, and (10) Hygiea. Comparisons are made with Earth- and space-based flux measurements that cover the infrared-to-centimeter wavelength spectrum. The models account for diurnal and seasonal effects as well as viewing geometry at the epochs of the observational data. Model fluxes at submillimeter and longer wavelengths are computed from a radiative transfer integral that takes into account temperature gradients in the subsurface and a plausible range of lunar-like electrical properties. A surface roughness model in the form of hemispherical mini-craters is included in the evaluation of the infrared flux comparisons.
Results of the infrared-to-centimeter comparisons confirm that low thermal inertia (I similar to 5-80 J/(K m(2) s(0.5))) material constitutes the upper similar to 1 cm of the four large asteroids studied. For the non-isothermal models considered, spectral emissivities near 1.0 fit the data of all four asteroids with no significant variations indicated throughout the infrared to microwave spectrum. Enhanced measured infrared flux levels (relative to a smooth surface model) of the four asteroids are constrained by a surface model with up to 50% fractional coverage of hemispherical craters, consistent with both the recent Lutetia result and historical measurements of the Moon's thermal flux characteristics. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Keihm, Stephen; Kamp, Lucas; Gulkis, Samuel; Hofstadter, Mark; Lee, Seungwon; Janssen, Michael; Choukroun, Mathieu] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Keihm, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM stephen.j.keihm@jpl.nasa.gov
RI Choukroun, Mathieu/F-3146-2017
OI Choukroun, Mathieu/0000-0001-7447-9139
FU National Aeronautics and Space Administration
FX This work has been conducted at the Jet Propulsion Laboratory,
California Institute and Technology, under a Contract with the National
Aeronautics and Space Administration.
NR 75
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U1 1
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 1086
EP 1102
DI 10.1016/j.icarus.2013.07.005
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200085
ER
PT J
AU Reddy, V
Li, JY
Le Corre, L
Scully, JEC
Gaskell, R
Russell, CT
Park, RS
Nathues, A
Raymond, C
Gaffey, MJ
Sierks, H
Becker, KJ
McFadden, LA
AF Reddy, Vishnu
Li, Jian-Yang
Le Corre, Lucille
Scully, Jennifer E. C.
Gaskell, Robert
Russell, Christopher T.
Park, Ryan S.
Nathues, Andreas
Raymond, Carol
Gaffey, Michael J.
Sierks, Holger
Becker, Kris J.
McFadden, Lucy A.
TI Comparing Dawn, Hubble Space Telescope, and ground-based interpretations
of (4) Vesta
SO ICARUS
LA English
DT Article
DE Asteroids, Rotation; Mineralogy; Asteroids, Surfaces; Asteroid Vesta;
Infrared observations
ID IAU/IAG WORKING GROUP; CARBONACEOUS CHONDRITE CLASTS; TRIAXIAL ELLIPSOID
DIMENSIONS; ADAPTIVE OPTICS IMAGES; ROTATIONAL ELEMENTS; REFLECTANCE
SPECTRA; COLOR VARIATIONS; MINOR PLANETS; ASTEROIDS; HETEROGENEITY
AB Observations of Asteroid (4) Vesta by NASA's Dawn spacecraft are interesting because its surface has the largest range of albedo, color and composition of any other asteroid visited by spacecraft to date. These hemispherical and rotational variations in surface brightness and composition have been attributed to impact processes since Vesta's formation. Prior to Dawn's arrival at Vesta, its surface properties were the focus of intense telescopic investigations for nearly a hundred years. Ground-based photometric and spectroscopic observations first revealed these variations followed later by those using Hubble Space Telescope (HST). Here we compare interpretations of Vesta's rotation period, pole, albedo, topographic, color, and compositional properties from ground-based telescopes and HST with those from Dawn. Our goal is to provide ground truth for prior interpretations and to help identify the limits of ground-based studies of asteroids in general. The improved rotational period measurement from Dawn is 0.222588652 day (Russell, C.T. et al. [2012]. Science 336, 684-686), and is consistent with the best ground-based rotation period of 0.22258874 day (Drummond, J.D., Fugate, R.Q., Christou, J.C. [1998]. Icarus 132, 80-99). The pole position for Vesta determined by Dawn is 309.03 degrees +/- 0.01 degrees, 42.23 degrees +/- 0.01 degrees and is within the uncertainties of pole orientation determined by Earth-based measurements (Li, J.-Y. et al. [2011]. Icarus 211, 528-534: 305.8 degrees +/- 3.1 degrees, 41.4 degrees +/- 1.5 degrees). Similarly, the obliquity of Vesta is 27.46 degrees based on the pole measurement from Dawn and all previous pole measurements put the obliquity within 3 degrees of this value. The topography range from the Dawn shape model is between -22.45 and +19.48 km relative to a 285 km x 285 km x 229 km ellipsoid. The HST range is slightly smaller (-12 km to +12 km relative to a 289 km x 280 km x 229 kin ellipsoid) than Dawn, likely due to lower spatial resolution of the former. We also present HST and Dawn albedo and color maps of Vesta in the Claudia (used by the Dawn team) and IAU coordinate systems. These maps serve to orient observers and identify compositional and albedo features from prior studies. We have linked several albedo features identified on HST maps to morphological features on Vesta using Dawn Framing Camera data. Rotational spectral variations observed from ground-based studies are also consistent with those observed by Dawn. While the interpretation of some of these features was tenuous from past data, the interpretations were reasonable given the limitations set by spatial resolution and our knowledge of Vesta and HED meteorites at that time. Our analysis shows that ground-based and HST observations are critical for our understanding of small bodies and provide valuable support for ongoing and future spacecraft missions. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Reddy, Vishnu; Li, Jian-Yang; Le Corre, Lucille; Gaskell, Robert] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany.
[Reddy, Vishnu; Le Corre, Lucille; Nathues, Andreas; Sierks, Holger] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Scully, Jennifer E. C.; Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Park, Ryan S.; Raymond, Carol] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gaffey, Michael J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
[Becker, Kris J.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[McFadden, Lucy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Reddy, V (reprint author), Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany.
EM reddy@psi.edu
OI McFadden, Lucy/0000-0002-0537-9975; Reddy, Vishnu/0000-0002-7743-3491;
Le Corre, Lucille/0000-0003-0349-7932
FU Max Planck Society; German Space Agency, DLR; NASA
FX We thank the Dawn team for the development, cruise, orbital insertion,
and operations of the Dawn spacecraft at Vesta. The Framing Camera
Project is financially supported by the Max Planck Society and the
German Space Agency, DLR. We also thank NASA's Dawn at Vesta
Participating Scientist Program for funding the research. A portion of
this work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA. Dawn data is archived
with the NASA Planetary Data System. VR would like to thank Juan Andreas
Sanchez and Guneshwar Singh Thangjam for their help in improving the
manuscript.
NR 65
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U1 0
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
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 1103
EP 1114
DI 10.1016/j.icarus.2013.07.019
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200086
ER
PT J
AU Goguen, JD
Buratti, BJ
Brown, RH
Clark, RN
Nicholson, PD
Hedman, MM
Howell, RR
Sotin, C
Cruikshank, DP
Baines, KH
Lawrence, KJ
Spencer, JR
Blackburn, DG
AF Goguen, Jay D.
Buratti, Bonnie J.
Brown, Robert H.
Clark, Roger N.
Nicholson, Phillip D.
Hedman, Matthew M.
Howell, Robert R.
Sotin, Christophe
Cruikshank, Dale P.
Baines, Kevin H.
Lawrence, Kenneth J.
Spencer, John R.
Blackburn, David G.
TI The temperature and width of an active fissure on Enceladus measured
with Cassini VIMS during the 14 April 2012 South Pole flyover
SO ICARUS
LA English
DT Article
DE Enceladus; Infrared observations; Geological processes; Satellites,
Surfaces; Saturn, Satellites
ID WATER RESERVOIR; ISS IMAGES; PLUME; FRACTURES; SURFACE; HYPOTHESIS;
JETS; HEAT
AB The width and temperature of the active fissures on Saturn's satellite Enceladus provide key observable constraints on physical models of these geyser-like eruptions. We analyze a sequence of high spatial resolution near-infrared spectra acquired with VIMS at 0.025 s intervals during a 74 km altitude flyover of the South Pole of Enceladus by the Cassini spacecraft on 14 April 2012 UTC. A thermal-emission spectrum covering 3- to 5-mu m wavelengths was detected as the field of view crossed one of the four major fissures, Baghdad Sulcus, within I km of 82.36S latitude and 28.24W longitude. We interpret this spectrum as thermal emission from a linear fissure with temperature 197 +/- 20 K and width 9 m. At the above wavelengths, the spectrum is dominated by the warmest temperature component. Looking downward into the fissure at only 13 degrees from the vertical, we conclude that our results measure the temperature of the interior fissure walls (and the H2O vapor) at depths within 40 m of the surface. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Goguen, Jay D.; Buratti, Bonnie J.; Howell, Robert R.; Sotin, Christophe; Baines, Kevin H.; Lawrence, Kenneth J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brown, Robert H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Clark, Roger N.] US Geol Survey, Lakewood, CO 80225 USA.
[Nicholson, Phillip D.; Hedman, Matthew M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Howell, Robert R.] Univ Wyoming, Dept Geol & Geophys, Laramie, WY 82071 USA.
[Cruikshank, Dale P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Spencer, John R.] Southwest Res Inst, Boulder, CO 80302 USA.
[Blackburn, David G.] Planetary Inst Space Res & Technol, Lowell, AR 72745 USA.
RP Goguen, JD (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-401,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Jay.D.Goguen@jpl.nasa.gov
FU Cassini Project at the Jet Propulsion Laboratory, California Institute
of Technology under National Aeronautics and Space Administration; NASA
Outer Planets Research Program
FX We acknowledge the Cassini Navigation Team and coordination with the
INMS and CIRS teams that enabled these observations. We are grateful to
the two anonymous referees for their insightful comments that improved
the final manuscript. This work was supported in part by the Cassini
Project at the Jet Propulsion Laboratory, California Institute of
Technology under a contract with the National Aeronautics and Space
Administration and in part by a grant from the NASA Outer Planets
Research Program.
NR 32
TC 19
Z9 19
U1 2
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
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 1128
EP 1137
DI 10.1016/j.icarus.2013.07.012
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200088
ER
PT J
AU Fernandez, YR
Kelley, MS
Lamy, PL
Toth, I
Groussin, O
Lisse, CM
A'Hearn, MF
Bauer, JM
Campins, H
Fitzsimmons, A
Licandro, J
Lowry, SC
Meech, KJ
Pittichova, J
Reach, WT
Snodgrass, C
Weaver, HA
AF Fernandez, Y. R.
Kelley, M. S.
Lamy, P. L.
Toth, I.
Groussin, O.
Lisse, C. M.
A'Hearn, M. F.
Bauer, J. M.
Campins, H.
Fitzsimmons, A.
Licandro, J.
Lowry, S. C.
Meech, K. J.
Pittichova, J.
Reach, W. T.
Snodgrass, C.
Weaver, H. A.
TI Thermal properties, sizes, and size distribution of Jupiter-family
cometary nuclei
SO ICARUS
LA English
DT Article
DE Comets, Nucleus; Comets, Dust; Infrared observations
ID SPITZER-SPACE-TELESCOPE; SHORT-PERIOD COMETS; NEAR-EARTH ASTEROIDS;
KUIPER-BELT OBJECTS; DEEP-IMPACT; CCD PHOTOMETRY; ENSEMBLE PROPERTIES;
RADAR OBSERVATIONS; DISTANT COMETS; 103P/HARTLEY 2
AB We present results from SEPPCoN, an on-going Survey of the Ensemble Physical Properties of Cometary Nuclei. In this report we discuss mid-infrared measurements of the thermal emission from 89 nuclei of Jupiter-family comets (JFCs). All data were obtained in 2006 and 2007 using imaging capabilities of the Spitzer Space Telescope. The comets were typically 4-5 AU from the Sun when observed and most showed only a point-source with little or no extended emission from dust. For those comets showing dust, we used image processing to photometrically extract the nuclei. For all 89 comets, we present new effective radii, and for 57 comets we present beaming parameters. Thus our survey provides the largest compilation of radiometrically-derived physical properties of nuclei to date. We have six main conclusions: (a) The average beaming parameter of the JFC population is 1.03 +/- 0.11, consistent with unity; coupled with the large distance of the nuclei from the Sun, this indicates that most nuclei have Tempel 1-like thermal inertia. Only two of the 57 nuclei had outlying values (in a statistical sense) of infrared beaming. (b) The known JFC population is not complete even at 3 km radius, and even for comets that approach to similar to 2 AU from the Sun and so ought to be more discoverable. Several recently-discovered comets in our survey have small perihelia and large (above similar to 2 km) radii. (c) With our radii, we derive an independent estimate of the JFC nuclear cumulative size distribution (CSD), and we find that it has a power-law slope of around -1.9, with the exact value depending on the bounds in radius. (d) This power-law is close to that derived by others from visible-wavelength observations that assume a fixed geometric albedo, suggesting that there is no strong dependence of geometric albedo with radius. (e) The observed CSD shows a hint of structure with an excess of comets with radii 3-6 km. (f) Our CSD is consistent with the idea that the intrinsic size distribution of the JFC population is not a simple power-law and lacks many sub-kilometer objects. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Fernandez, Y. R.; Campins, H.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Kelley, M. S.; A'Hearn, M. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Lamy, P. L.; Toth, I.; Groussin, O.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille UMR 7326, F-13388 Marseille, France.
[Toth, I.] Konkoly Observ MTA CSFK CSI, H-1525 Budapest, Hungary.
[Lisse, C. M.; Weaver, H. A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Bauer, J. M.; Pittichova, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Fitzsimmons, A.] Queens Univ Belfast, Sch Phys & Astron, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Licandro, J.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Lowry, S. C.] Univ Kent, Sch Phys Sci, Canterbury CT2 7NH, Kent, England.
[Meech, K. J.] Univ Hawaii, Inst Astron, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
[Reach, W. T.] NASA, Stratospher Observ Infrared Astron, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Snodgrass, C.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
RP Fernandez, YR (reprint author), Univ Cent Florida, Dept Phys, 4000 Cent Florida Blvd, Orlando, FL 32816 USA.
EM yan@physics.ucf.edu
RI Lisse, Carey/B-7772-2016;
OI Lisse, Carey/0000-0002-9548-1526; Fernandez, Yanga/0000-0003-1156-9721;
Kelley, Michael/0000-0002-6702-7676; Reach, William/0000-0001-8362-4094;
Snodgrass, Colin/0000-0001-9328-2905
FU NASA; NASA through JPL/Caltech, RSA [1289123]; NASA [NNX-09AB44G];
National Science Foundation [AST-0808004]; European Union Seventh
Framework Programme [268421]
FX We are grateful for the recommendations and suggestions to this
manuscript made by Olivier Hainaut and one anonymous referee. 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, RSA #1289123,
to Y.R.F. and H.C. Support for this work also came from NASA through
Grant NNX-09AB44G to Y.R.F., S.C.L., K.J.M., and J.M.B.; from the
National Science Foundation through Grant AST-0808004 to Y.R.F., S.C.L.,
and K.J.M.; and from the European Union Seventh Framework Programme
(FP7/2007-2013) under Grant Agreement No. 268421 to C.S.
NR 90
TC 24
Z9 24
U1 1
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 1138
EP 1170
DI 10.1016/j.icarus.2013.07.021
PG 33
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200089
ER
PT J
AU Cataldo, E
Davies, AG
Wilson, L
AF Cataldo, Enzo
Davies, Ashley Gerard
Wilson, Lionel
TI Near-vertical supersonic and shock-free gas/magma flow at ionian
volcanoes: Application to Pillan
SO ICARUS
LA English
DT Article
DE Io; Volcanism; Geological processes; Jupiter, Satellites
ID ERUPTION; IO; MAGMA; EMPLACEMENT; TVASHTAR; GALILEO; STYLE; PELE; MOON
AB In 1997, the Pillan volcano on Io was home to a fierce volcanic eruption that emplaced extensive lava flows and a circular plume deposit. The gas/magma flow issuing from the unresolved vent region appeared to form an almost vertical jet. We consider steady eruptions of gas and magma, and take the vent to be either a fissure or a point source. In the fissure scenario, the upper-conduit flow must reach Mach 1 in the 25-75 m depth range to produce the vent velocities of 550-600 m/s that are required to explain the observed plume heights. Conduit wall deflections in the range 20-30 degrees from vertical (values referring to the upper meter of the conduit) and similar to 26-30% by mass of incorporated crustal SO2 are also needed. In the point-source scenario, sonic flow conditions and similar velocities are achieved in the depth range 350-500 m for similar conduit wall deflections and gas mass proportions in the erupting mixture. Probably, the source of the 140-km-high plume imaged in 1997 was either a similar to 6-11 m-wide fissure, active for similar to 14-40 km along strike, or a circular vent similar to 125-216 m in diameter, the former scenario being preferred. Finally, a shock-free conduit flow is more likely to sustain a tall lava fountain in a near-vacuum. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Cataldo, Enzo] Univ Milano Bicocca, Dipartimento Geol & Geotecnol, IT-20126 Milan, Italy.
[Cataldo, Enzo] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England.
[Wilson, Lionel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Davies, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Ashley.Davies@jpl.nasa.gov
FU NASA Geology and Geophysics Program
FX We are grateful for the constructive comments of reviewers. AGD is
supported by a grant from the NASA Geology and Geophysics Program. Part
of this work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract to NASA. (C)2013 Caltech. All
rights reserved.
NR 23
TC 0
Z9 0
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
J9 ICARUS
JI Icarus
PD SEP-OCT
PY 2013
VL 226
IS 1
BP 1171
EP 1176
DI 10.1016/j.icarus.2013.06.035
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 222GW
UT WOS:000324720200090
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Untitled
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] CALTECH, Pasadena, CA 91125 USA.
CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Siegel, Peter H.] IRMMW THz, Pasadena, CA USA.
RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM phs@caltech.edu
NR 0
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 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD SEP
PY 2013
VL 3
IS 5
BP 501
EP 504
DI 10.1109/TTHZ.2013.2275914
PG 4
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 225HY
UT WOS:000324954300001
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneers A Series of Interviews With Significant Contributors
to Terahertz Science and Technology
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91109 USA.
[Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91109 USA.
[Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91109 USA.
NR 0
TC 0
Z9 0
U1 1
U2 6
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 SEP
PY 2013
VL 3
IS 5
BP 505
EP 505
DI 10.1109/TTHZ.2013.2272655
PG 1
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 225HY
UT WOS:000324954300002
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneer: Fritz Keilmann "RF Biophysics: From Strong Field to
Near Field"
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
ID INFRARED NONLINEAR OPTICS; ELASTIC LIGHT-SCATTERING; P-TYPE GERMANIUM;
SPATIAL-RESOLUTION; YEAST GROWTH; SUBWAVELENGTH RESOLUTION;
ABSORPTION-SPECTROSCOPY; MICROWAVE-FREQUENCIES; MOBILE CARRIERS;
MICROSCOPY
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA.
[Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
[Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA.
EM phs@caltech.edu
NR 118
TC 0
Z9 0
U1 4
U2 20
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 SEP
PY 2013
VL 3
IS 5
BP 506
EP 514
DI 10.1109/TTHZ.2013.2272656
PG 9
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 225HY
UT WOS:000324954300003
ER
PT J
AU Llombart, N
Lee, C
Alonso-delPino, M
Chattopadhyay, G
Jung-Kubiak, C
Jofre, L
Mehdi, I
AF Llombart, N.
Lee, C.
Alonso-delPino, M.
Chattopadhyay, G.
Jung-Kubiak, C.
Jofre, L.
Mehdi, I.
TI Silicon Micromachined Lens Antenna for THz Integrated Heterodyne Arrays
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Lens; leaky wave antennas; silicon fabrication; terahertz (THz)
ID TERAHERTZ; RADAR
AB In this paper, we present the design, fabrication, and measurements of a lens THz antenna that can be fabricated using conventional photolithography and deep reactive etching processes. The antenna is composed of an extended hemispherical silicon lens and a leaky wave waveguide feed. Both elements are fabricated using silicon micromachining techniques, enabling the fabrication of future large antenna arrays with a parallel process. To show the concept, a first antenna prototype has been fabricated using this fabrication process. Measurements obtained at 550 GHz are presented.
C1 [Llombart, N.] Univ Complutense Madrid, Dept Opt, E-28040 Madrid, Spain.
[Alonso-delPino, M.; Jofre, L.] Tech Univ Catalonia, Signal Theory & Commun Dept, Barcelona 08034, Spain.
[Lee, C.; Chattopadhyay, G.; Jung-Kubiak, C.; Mehdi, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Llombart, N (reprint author), Delft Univ Technol, NL-2628 AZ Delft, Netherlands.
EM maria.alonso@tsc.upc.edu
RI Jofre, Lluis/E-5879-2013
OI Jofre, Lluis/0000-0002-0547-901X
FU Jet Propulsion Laboratory, California Institute of Technology, Pasadena,
CA, USA; National Aeronautics and Space Administration; Spanish CICYT
[AYA2010-10054-E, TEC2007-66698-C04-01, TEC2010-20841-C04-02]; program
"Ramon y Cajal" [RYC-2009-04924]; CONSOLIDER [CSD2008-68]
FX Manuscript received February 25, 2013; revised May 06, 2013; accepted
June 05, 2013. Date of publication July 15, 2013; date of current
version September 18, 2013. This work was supported in part by the Jet
Propulsion Laboratory, California Institute of Technology, Pasadena, CA,
USA, under a contract with the National Aeronautics and Space
Administration. The work of N. Llombart was supported by the Spanish
CICYT under Grant AYA2010-10054-E and by the program "Ramon y Cajal"
RYC-2009-04924. The work of M. Alonso-delPino was supported by the
Spanish CICYT under Grants TEC2007-66698-C04-01, TEC2010-20841-C04-02,
and CONSOLIDER CSD2008-68.
NR 19
TC 14
Z9 14
U1 3
U2 22
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 SEP
PY 2013
VL 3
IS 5
BP 515
EP 523
DI 10.1109/TTHZ.2013.2270300
PG 9
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 225HY
UT WOS:000324954300004
ER
PT J
AU Leal-Sevillano, CA
Cooper, KB
Ruiz-Cruz, JA
Montejo-Garai, JR
Rebollar, JM
AF Leal-Sevillano, Carlos A.
Cooper, Ken B.
Ruiz-Cruz, Jorge A.
Montejo-Garai, Jose R.
Rebollar, Jesus M.
TI A 225 GHz Circular Polarization Waveguide Duplexer Based on a Septum
Orthomode Transducer Polarizer
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Circular polarization; duplexer; orthomode transducer; terahertz
ID DUAL-POLARIZATION; ANTENNA FEEDERS; MILLIMETER-WAVE; BAND; DESIGN; HORN;
OPTIMIZATION; RADIATION; COMPACT; RADAR
AB In this paper, we present the modeling and experimental validation of an efficient, compact, and high-isolation waveguide duplexer operating at 225 GHz. While duplexers based on ferrite circulators are key components of many monostatic radar systems, at W-band frequencies and above the performance of waveguide circulators rapidly deteriorates. The design presented here uses a ferrite-free duplexing concept based on transmitting and receiving in orthogonal circular polarizations. The circular polarization is efficiently generated in waveguide using a septum orthomode transducer polarizer, leading to a compact device with a single horn antenna. The complete duplexer is designed using efficient numerical algorithms, resulting in a fabricated device with a measured 10% fractional bandwidth, a return loss better than 20 dB, isolation of 30 dB, and insertion loss below 1 dB.
C1 [Leal-Sevillano, Carlos A.; Montejo-Garai, Jose R.; Rebollar, Jesus M.] Univ Politecn Madrid, ETSI Telecomunicac, Dept Electromagnetismo & Teoria Circuitos, E-28040 Madrid, Spain.
[Cooper, Ken B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ruiz-Cruz, Jorge A.] Univ Autonoma Madrid, Escuela Politecn Super, E-28049 Madrid, Spain.
RP Leal-Sevillano, CA (reprint author), Univ Politecn Madrid, ETSI Telecomunicac, Dept Electromagnetismo & Teoria Circuitos, E-28040 Madrid, Spain.
EM caleal@etc.upm.es
RI Ruiz-Cruz, Jorge/C-8159-2014
OI Ruiz-Cruz, Jorge/0000-0003-3909-8263
FU National Aeronautics and Space Administration; Spanish government
program [TEC2010-17795]; Universidad Politecnica de Madrid, Madrid,
Spain; [CSD2008-00068]
FX This work was in part carried out at the Jet Propulsion Laboratory,
California Institute of Technology, Pasadena, CA, under a contract with
the National Aeronautics and Space Administration. This work was
supported in part by the Spanish government program TEC2010-17795, the
CONSOLIDER CSD2008-00068, and by a Ph.D. grant from Universidad
Politecnica de Madrid, Madrid, Spain.
NR 52
TC 6
Z9 6
U1 2
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 SEP
PY 2013
VL 3
IS 5
BP 574
EP 583
DI 10.1109/TTHZ.2013.2264317
PG 10
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 225HY
UT WOS:000324954300011
ER
PT J
AU Korolev, A
Strapp, JW
Isaac, GA
Emery, E
AF Korolev, A.
Strapp, J. W.
Isaac, G. A.
Emery, E.
TI Improved Airborne Hot-Wire Measurements of Ice Water Content in Clouds
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
DE Aircraft observations; In situ atmospheric observations;
Instrumentation; sensors
ID COUNTERFLOW VIRTUAL IMPACTOR; PART I; PROBE; PERFORMANCE; CALIBRATION;
MASSES
AB Airborne measurements of ice water content (IWC) in both ice and mixed-phase clouds remain one of the long-standing problems in experimental cloud physics. For nearly three decades, IWC has been measured with the help of the Nevzorov hot-wire total water content (TWC) sensor, which had an inverted cone shape. It was assumed that ice particles would be captured inside the cone and then completely melt and evaporate. However, wind tunnel experiments conducted with the help of high-speed video recordings showed that ice particles may bounce out of the TWC cone, resulting in the underestimation of the measured IWC. The TWC sensor was modified to improve the capture efficiency of ice particles. The modified sensor was mounted on the National Research Council (NRC) Convair-580 and its measurements in ice clouds were compared with the measurements of the original Nevzorov TWC sensor, a Droplet Measurement Technologies (DMT) counterflow virtual impactor (CVI), and IWC calculated from the particle size distribution measured by optical array probes (OAPs). Results indicated that the IWC measured by the modified TWC hot-wire sensor as well as the CVI and that deduced from the OAP size distributions agreed reasonably well when the maximum size of ice particles did not exceed 4 mm. However, IWC measured by the original TWC sensor was approximately 3 times lower than that measured by the other three techniques. This result can be used for the retrieval of the past IWC measurements obtained with this TWC sensor. For clouds with ice particles larger than 4 mm, the IWC measured by the modified TWC sensor and CVI exhibited diverging measurements.
C1 [Korolev, A.; Strapp, J. W.; Isaac, G. A.] Environm Canada, Cloud Phys & Severe Weather Res Sect, Toronto, ON M3H 5T4, Canada.
[Emery, E.] NASA Glenn Res Ctr, Cleveland, OH USA.
RP Korolev, A (reprint author), Environm Canada, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada.
EM alexei.korolev@ec.gc.ca
FU Canadian Space Agency (CSA); Transport Canada
FX Many thanks are given to Vincent Reich from NASA Glenn for providing the
high-speed video equipment during the Cox & Co. wind tunnel tests and
the in situ sampling on the NRC Convair-580. The aircraft data were
obtained using the NRC Convair-580 and the scientific and technical
efforts of many NRC and MSC staff. A special thanks is given to the Cox
& Co. personnel and, in particular, to Adam Lawrence for a high level of
cooperation and support in operating the Cox & Co. wind tunnel facility.
The Canadian Space Agency (CSA) provided funding for the C3VP aircraft
projects. The Federal Aviation Administration as well as NASA Glenn
provided support for the in situ measurements in 2004. Transport Canada
has provided support for all of this work. The authors also express
their gratitude to three anonymous reviewers for their thoughtful
comments and valuable suggestions.
NR 29
TC 7
Z9 8
U1 0
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD SEP
PY 2013
VL 30
IS 9
BP 2121
EP 2131
DI 10.1175/JTECH-D-13-00007.1
PG 11
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 224MH
UT WOS:000324890100012
ER
PT J
AU Liu, D
Khaykovich, B
Gubarev, MV
Robertson, JL
Crow, L
Ramsey, BD
Moncton, DE
AF Liu, Dazhi
Khaykovich, Boris
Gubarev, Mikhail V.
Robertson, J. Lee
Crow, Lowell
Ramsey, Brian D.
Moncton, David E.
TI Demonstration of a novel focusing small-angle neutron scattering
instrument equipped with axisymmetric mirrors
SO NATURE COMMUNICATIONS
LA English
DT Article
ID REFRACTIVE OPTICS; RESOLUTION; DIFFRACTOMETER; CALIBRATION; FLUX
AB Small-angle neutron scattering (SANS) is the most significant neutron technique in terms of impact on science and engineering. However, the basic design of SANS facilities has not changed since the technique's inception about 40 years ago, as all SANS instruments, save a few, are still designed as pinhole cameras. Here we demonstrate a novel concept for a SANS instrument based on axisymmetric focusing mirrors. We build and test a small prototype, which shows a performance comparable to that of conventional large SANS facilities. By using a detector with 48-mu m pixels, we build the most compact SANS instrument in the world. This work, together with the recent demonstration that such mirrors could increase the signal rate at least 50-fold, for large samples, while improving resolution, paves the way to novel SANS instruments, thus affecting a broad community of scientists and engineers.
C1 [Liu, Dazhi; Khaykovich, Boris; Moncton, David E.] MIT, Nucl Reactor Lab, Cambridge, MA 02139 USA.
[Gubarev, Mikhail V.; Ramsey, Brian D.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Robertson, J. Lee; Crow, Lowell] Oak Ridge Natl Lab, Instrument & Source Design Div, Oak Ridge, TN 37831 USA.
[Moncton, David E.] MIT, Dept Phys, Cambridge, MA 02139 USA.
RP Khaykovich, B (reprint author), MIT, Nucl Reactor Lab, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM bkh@mit.edu
RI Liu, Dazhi/G-2675-2013; Khaykovich, Boris/A-7376-2012
OI Liu, Dazhi/0000-0002-7604-6940; Khaykovich, Boris/0000-0002-9490-2771
FU US Department of Energy, Office of Basic Energy Sciences, Division of
Materials Sciences and Engineering [DE-FG02-09ER46556,
DE-FG02-09ER46557]; Basic Energy Science (BES) Program, Office of
Science, US Department of Energy [DE-AC05-00OR22725]; UT-Battelle, LLC
FX We acknowledge useful discussions with Dr. D.F.R. Mildner (NIST).
Research has been supported by the US Department of Energy, Office of
Basic Energy Sciences, Division of Materials Sciences and Engineering
under Awards no. DE-FG02-09ER46556 and no. DE-FG02-09ER46557. The work
at ORNL has been sponsored by the Basic Energy Science (BES) Program,
Office of Science, US Department of Energy under contract number
DE-AC05-00OR22725 with UT-Battelle, LLC.
NR 24
TC 9
Z9 9
U1 0
U2 25
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 SEP
PY 2013
VL 4
AR 2556
DI 10.1038/ncomms3556
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 233BD
UT WOS:000325538300001
PM 24077533
ER
PT J
AU Seshadri, S
Shapiro, C
Goodsall, T
Fucik, J
Hirata, C
Rhodes, JD
Rowe, BTP
Smith, RM
AF Seshadri, S.
Shapiro, C.
Goodsall, T.
Fucik, J.
Hirata, C.
Rhodes, J. D.
Rowe, B. T. P.
Smith, R. M.
TI Initial Results from a Laboratory Emulation of Weak Gravitational
Lensing Measurements
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE Astronomical Techniques
ID SELECTION; IMAGES; COSMOS; SPACE
AB Weak gravitational lensing observations are a key science driver for the NASA Wide Field Infrared Survey Telescope (WFIRST). To validate the performance of the WFIRST infrared detectors, we have performed a laboratory emulation of weak gravitational lensing measurements. Our experiments used a custom precision projector system to image a target mask composed of a grid of pinholes, emulating stellar point sources, onto a 1.7m cut-off Teledyne HgCdTe/H2RG detector. We used a 0.88m LED illumination source and f/22 pupil stop to produce undersampled point spread functions similar to those expected from WFIRST. We also emulated the WFIRST image reconstruction strategy, using the image combination (IMCOM) algorithm to derive oversampled images from dithered, undersampled input images. We created shear maps for this data and computed shear correlation functions to mimic a real weak lensing analysis. After removing only second-order polynomial fits to the shear maps, we found that the correlation functions could be reduced to O(10(-6)). This places a conservative upper limit on the detector-induced bias to the correlation function (under our test conditions). This bias is two orders of magnitude lower than the expected weak lensing signal. Restricted to scales relevant to dark energy analyses (sky separations >0.5), the bias is O(10(-7))comparable to the requirement for future weak lensing missions to avoid biasing cosmological parameter estimates. Our experiment will need to be upgraded and repeated under different configurations to fully characterize the shape measurement performance of WFIRST IR detectors.
C1 [Seshadri, S.; Shapiro, C.; Goodsall, T.; Rhodes, J. D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Fucik, J.; Hirata, C.; Rhodes, J. D.; Smith, R. M.] CALTECH, Pasadena, CA 91125 USA.
[Rowe, B. T. P.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
RP Seshadri, S (reprint author), CALTECH, Jet Prop Lab, MS 300-315,4800 Oak Grove Dr, Pasadena, CA USA.
EM suresh.seshadri@jpl.nasa.gov
OI Rowe, Barnaby/0000-0002-7042-9174
FU National Aeronautics and Space Administration; internal JPL Research and
Technology Development (RTD) program; Director's Research Development
Fund (DRDF) program; US Department of Energy's (DOE) Supernova
Acceleration Probe (SNAP) project; US Department of Energy's (DOE) Joint
Dark Energy Mission (JDEM) project; NASA Wide Field IR Survey Telescope
(WFIRST) project office; NASA Joint Dark Energy Mission (JDEM) project
office; NASA Post-doctoral Program Fellowship Program from Oak Ridge
Associated Universities; European Research Council [240672]
FX This research was carried out at the Jet Propulsion Laboratory and
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. We are grateful to the following
organizations and programs for their support of this effort: internal
JPL Research and Technology Development (RTD) and Director's Research
Development Fund (DRDF) programs; US Department of Energy's (DOE)
Supernova Acceleration Probe (SNAP) and Joint Dark Energy Mission (JDEM)
projects; the NASA Wide Field IR Survey Telescope (WFIRST) and Joint
Dark Energy Mission (JDEM) project offices. CS acknowledges support from
the NASA Post-doctoral Program Fellowship Program from Oak Ridge
Associated Universities. BR acknowledges support from European Research
Council in the form of a Starting Grant with number 240672.
NR 48
TC 3
Z9 3
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP 1
PY 2013
VL 125
IS 931
BP 1065
EP 1086
DI 10.1086/673318
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 223VD
UT WOS:000324838700004
ER
PT J
AU Santamarta, R
Arroyave, R
Pons, J
Evirgen, A
Karaman, I
Karaca, HE
Noebe, RD
AF Santamarta, R.
Arroyave, R.
Pons, J.
Evirgen, A.
Karaman, I.
Karaca, H. E.
Noebe, R. D.
TI TEM study of structural and micro structural characteristics of a
precipitate phase in Ni-rich Ni-Ti-Hf and Ni-Ti-Zr shape memory alloys
SO ACTA MATERIALIA
LA English
DT Article
DE High-temperature shape memory alloys; Precipitation; Martensitic
transformation; DFT calculations; NiTiZr
ID BRILLOUIN-ZONE INTEGRATIONS; TOTAL-ENERGY CALCULATIONS; WAVE BASIS-SET;
MARTENSITIC-TRANSFORMATION; MECHANICAL-BEHAVIOR; ELECTRON-MICROSCOPY;
TEMPERATURE; MICROSTRUCTURE; CRYSTALLIZATION; METALS
AB The precipitates formed after suitable thermal treatments in seven Ni-rich Ni-Ti-Hf and Ni-Ti-Zr high-temperature shape memory alloys have been investigated by conventional and high-resolution transmission electron microscopy. In both ternary systems, the precipitate coarsening kinetics become faster as the Ni and ternary element contents (Hf or Zr) of the bulk alloy are increased, in agreement with the precipitate composition measured by energy-dispersive X-ray microanalysis. The precipitate structure has been found to be the same in both Hf- and Zr-containing ternary alloys, and determined to be a superstructure of the B2 austenite phase, which arises from a recombination of the Hf/Zr and Ti atoms in their sublattice. Two different structural models for the precipitate phase were optimized using density functional theory methods. These calculations indicate that the energetics of the structure are not very sensitive to the atomic configuration of the Ti Hf/Zr planes, thus significant configurational disorder due to entropic effects can be envisaged at high temperatures. The precipitates are fully coherent with the austenite B2 matrix; however, upon martensitic transformation, they lose some coherency with the B19' matrix as a result of the transformation shear process in the surrounding matrix. The strain accommodation around the particles is much easier in the Ni Ti Zr-containing alloys than in the Ni Ti Hf system, which correlates well with the lower transformation strain and stiffness predicted for the Ni Ti Zr alloys. The B19' martensite twinning modes observed in the studied Ni-rich ternary alloys are not changed by the new precipitated phase, being equivalent to those previously reported in Ni-poor ternary alloys. (C) 2013 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Santamarta, R.; Pons, J.] Univ Illes Balears, Dept Fis, E-07122 Palma De Mallorca, Spain.
[Arroyave, R.; Evirgen, A.; Karaman, I.] Texas A&M Univ, Dept Mat Sci & Engn, College Stn, TX 77843 USA.
[Arroyave, R.; Karaman, I.] Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA.
[Karaca, H. E.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Noebe, R. D.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Santamarta, R (reprint author), Univ Illes Balears, Dept Fis, E-07122 Palma De Mallorca, Spain.
EM ruben.santamarta@uib.es
RI Karaman, Ibrahim/E-7450-2010; Santamarta, Ruben/K-7865-2016
OI Karaman, Ibrahim/0000-0001-6461-4958; Santamarta,
Ruben/0000-0003-3341-5758
FU Spanish MINECO; FEDER [MAT2011-28217-C02-01]; US Air Force Office of
Scientific Research [FA9550-12-1-0218]; NASA EPSCOR [NNX11AQ31A];
National Science Foundation [DMR 08-44082]; NASA Fundamental Aeronautics
Program, Aeronautical Sciences Project; [NSF-CMMI-0953984]
FX Partial financial support from Spanish MINECO and FEDER under Project
Number MAT2011-28217-C02-01 is acknowledged. The work was also supported
by the US Air Force Office of Scientific Research, under Grant No.
FA9550-12-1-0218 and NASA EPSCOR program under Grant No. NNX11AQ31A.
Additional support was received by the National Science Foundation under
Grant No. DMR 08-44082, which supports the International Materials
Institute for Multi-functional Materials for Energy Conversion (IIMEC)
at Texas A&M University. R.D.N. gratefully acknowledges support from the
NASA Fundamental Aeronautics Program, Aeronautical Sciences Project.
R.A. also acknowledges the support from the Grant NSF-CMMI-0953984.
First-principles calculations were carried out in the Chemical
Engineering cluster of Texas A&M University, the Texas A&M
Supercomputing facility, and the Ranger and Lonestar clusters at the
Texas Advanced Computing Center (TACC) in the University of Texas at
Austin.
NR 52
TC 32
Z9 33
U1 5
U2 66
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 SEP
PY 2013
VL 61
IS 16
BP 6191
EP 6206
DI 10.1016/j.actamat.2013.06.057
PG 16
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA 218RI
UT WOS:000324449700024
ER
PT J
AU Lane, HW
Bourland, C
Barrett, A
Heer, M
Smith, SM
AF Lane, Helen W.
Bourland, Charles
Barrett, Ann
Heer, Martina
Smith, Scott M.
TI The Role of Nutritional Research in the Success of Human Space Flight
SO ADVANCES IN NUTRITION
LA English
DT Editorial Material
CT Symposium on the Role of Nutritional Research in the Success of Human
Space Flight held at the ASN Scientific Sessions and Annual Meeting at
Experimental Biology
CY APR 23, 2013
CL Boston, MA
SP Amer Soc Nutr, Amer Soc Nutr Hist Nutr Comm
ID LONG-DURATION SPACEFLIGHT; BONE-RESORPTION
AB The United States has had human space flight programs for >50 y and has had a continued presence in space since 2000. Providing nutritious and safe food is imperative for astronauts because space travelers are totally dependent on launched food. Space flight research topics have included energy, protein, nutritional aspects of bone and muscle health, and vision issues related to 1-carbon metabolism. Research has shown that energy needs during flight are similar to energy needs on Earth. Low energy intakes affect protein turnover. The type of dietary protein is also important for bone health, plant-based protein being more efficacious than animal protein. Bone loss is greatly ameliorated with adequate intakes of energy and vitamin D, along with routine resistive exercise. Astronauts with lower plasma folate concentrations may be more susceptible to vision changes. Foods for space flight were developed initially by the U.S. Air Force School of Aerospace Medicine in conjunction with the U.S. Army Natick Laboratories and NASA. Hazard Analysis Critical Control Point safety standards were specifically developed for space feeding. Prepackaged foods for the International Space Station were originally high in sodium (5300 mg/d), but NASA has recently reformulated >90 foods to reduce sodium intake to 3000 mg/d. Food development has improved nutritional quality as well as safety and acceptability.
C1 [Lane, Helen W.; Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Human Hlth & Performance Directorate, Houston, TX 77058 USA.
[Bourland, Charles] NASA, Houston, TX USA.
[Barrett, Ann] US Army Natick Soldier Res Dev & Engn Ctr, Combat Feeding Directorate, Natick, MA USA.
[Heer, Martina] Profil, Neuss, Germany.
[Heer, Martina] Univ Bonn, Dept Food & Nutr Sci, Bonn, Germany.
RP Lane, HW (reprint author), NASA, Lyndon B Johnson Space Ctr, Human Hlth & Performance Directorate, Houston, TX 77058 USA.
NR 9
TC 3
Z9 6
U1 4
U2 18
PU AMER SOC NUTRITION-ASN
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 2161-8313
EI 2156-5376
J9 ADV NUTR
JI Adv. Nutr.
PD SEP
PY 2013
VL 4
IS 5
BP 521
EP 523
DI 10.3945/an.113.004101
PG 3
WC Nutrition & Dietetics
SC Nutrition & Dietetics
GA 217KH
UT WOS:000324357900004
PM 24038244
ER
PT J
AU Harris, L
Tozzi, S
Wiley, P
Young, C
Richardson, TMJ
Clark, K
Trent, JD
AF Harris, Linden
Tozzi, Sasha
Wiley, Patrick
Young, Colleen
Richardson, Tra-My Justine
Clark, Kit
Trent, Jonathan D.
TI Potential impact of biofouling on the photobioreactors of the Offshore
Membrane Enclosures for Growing Algae (OMEGA) system
SO BIORESOURCE TECHNOLOGY
LA English
DT Article
DE Photobioreactor; Biofouling; OMEGA; Algae; Biofuels
ID WASTE-WATER TREATMENT; EELGRASS ZOSTERA-MARINA; LIGHT ATTENUATION;
COATINGS; BIOFILMS; MICROALGAE; SURFACES; BIOFUELS
AB The influence of PBR composition [clear polyurethane (PolyU) vs. clear linear low-density polyethylene (LLDPE) (top) and black opaque high-density polyethylene (bottom)] and shape (rectangular vs. tubular) on biofouling and the influence of biofouling on algae productivity were investigated. In 9-week experiments, PBR biofouling was dominated by pennate diatoms and clear plastics developed macroalgae. LLDPE exhibited lower photosynthetic-active-radiation (PAR) light transmittance than PolyU before biofouling, but higher transmittance afterwards. Both rectangular and tubular LLDPE PBRs accumulated biofouling predominantly along their wetted edges. For a tubular LLDPE PBR after 12 weeks of biofouling, the correlation between biomass, percent surface coverage, and PAR transmittance was complex, but in general biomass inversely correlated with transmittance. Wrapping segments of this biofouled LLDPE around an algae culture reduced CO2 and NH3-N utilization, indicating that external biofouling must be controlled. (C) 2013 The Authors. Published by Elsevier Ltd. All rights reserved.
C1 [Harris, Linden; Wiley, Patrick; Richardson, Tra-My Justine] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Tozzi, Sasha] Univ Calif Santa Cruz, Dept Ocean Sci, Santa Cruz, CA 95064 USA.
[Wiley, Patrick] Univ Calif Merced Sch Engn, Merced, CA 95343 USA.
[Trent, Jonathan D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Young, Colleen] Calif Dept Fish & Wildlife, Santa Cruz, CA 95060 USA.
[Clark, Kit] SETI, Mountain View, CA 94043 USA.
RP Trent, JD (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Jonathan.D.Trent@nasa.gov
FU NASA; California Energy Commission-PIER
FX The authors thank S. Harmsen, W. Fennie, M. Cruickshank, J. Kuo, B.
Smith, and S. Ord for field assistance, T. Embaye, S. Reinsch, and S.
Zimmerman for lab assistance; S. Fauth and B. McKuin for editing; D.
Jessup, M. Miller, S. Lamerdin and J. Douglas for access to lab and
field sites. NASA and the California Energy Commission-PIER provided
funding.
NR 35
TC 9
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U1 7
U2 60
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0960-8524
J9 BIORESOURCE TECHNOL
JI Bioresour. Technol.
PD SEP
PY 2013
VL 144
BP 420
EP 428
DI 10.1016/j.biortech.2013.06.125
PG 9
WC Agricultural Engineering; Biotechnology & Applied Microbiology; Energy &
Fuels
SC Agriculture; Biotechnology & Applied Microbiology; Energy & Fuels
GA 216JS
UT WOS:000324280100057
PM 23907145
ER
PT J
AU Volkov, DL
Landerer, FW
Kirillov, SA
AF Volkov, Denis L.
Landerer, Felix W.
Kirillov, Sergey A.
TI The genesis of sea level variability in the Barents Sea
SO CONTINENTAL SHELF RESEARCH
LA English
DT Article
DE Barents Sea; Sea level variability; Satellite altimetry; GRACE; ECCO2;
Arctic seas
ID OCEAN; GRACE; MODEL
AB The regional variability of sea level is an integral indicator of changing oceanographic conditions due to different processes of oceanic, atmospheric, and terrestrial origin. The present study explores the nature of sea level variability in the Barents Sea a marginal shelf sea of the Arctic Ocean. A characteristic feature that distinguishes this sea from other Arctic shelf seas is that it is largely ice free throughout the year. This allows continuous monitoring of sea level by space-borne altimeters. In this work we combine satellite altimetry, ocean gravity measurements by GRACE satellites, available hydrography data, and a high-resolution ocean data synthesis product to estimate the steric and mass-related components of sea level in the Barents Sea. We present one of the first observational evidence of the local importance of the mass-related sea level changes. The observed 1-3 month phase lag between the annual cycles of sea level in the Barents Sea and in the Nordic seas (Norwegian, Iceland, Greenland seas) is explained by the annual mass-related changes. The analysis of the barotropic vorticity budget shows that the mass-related sea level variability in the central part of the Barents Sea is determined by the combined effect of wind stress, flow over the varying bottom topography, and dissipation, while the impact of vorticity fluxes is negligible. Overall, the steric sea level has smaller amplitudes and mainly varies on the seasonal time scale. The thermosteric sea level is the main contributor to the steric sea level along the pathways of the Atlantic inflow into the Barents Sea. The relative contribution of the halosteric sea level is dominant in the southeastern, eastern, and northern parts of the Barents Sea, modulated by the seasonal sea ice formation/melt as well as by continental runoff. The variability of the thermosteric sea level in the Barents Sea is mostly driven by variations in the net surface heat flux, whereas the contribution of heat advection becomes as important as the ocean-atmosphere heat exchange at interannual time scales. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Volkov, Denis L.] Univ Miami, Cooperat Inst Marine & Atmospher Studies, Miami, FL USA.
[Volkov, Denis L.] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA.
[Landerer, Felix W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kirillov, Sergey A.] Arctic & Antarctic Res Inst, St Petersburg 199226, Russia.
[Kirillov, Sergey A.] St Petersburg State Univ, Dept Oceanol, St Petersburg 199034, Russia.
RP Volkov, DL (reprint author), NOAA, Atlantic Oceanog & Meteorol Lab, PhOD, 4301 Rickenbacker Causeway, Miami, FL 33149 USA.
EM Denis.Volkov@noaa.gov
RI Volkov, Denis/A-6079-2011;
OI Volkov, Denis/0000-0002-9290-0502; Landerer, Felix/0000-0003-2678-095X
FU CNES; NASA MEASURES Program; NASA Physical Oceanography program; Russian
Federal Targeted program
FX The altimeter products were produced by SSALTO/DUACS and distributed by
AVISO with support from CNES (http://www.aviso.oceanobs.com/duacs/).
GRACE ocean data were processed by Don R Chambers, supported by the NASA
MEASURES Program, and are available at http://grace.jpl.nasa.gov. The
authors thank two anonymous reviewers for their comments and suggestions
that helped to improve the manuscript. The ECCO2 model runs have been
carried out at Jet Propulsion Laboratory, California Institute of
Technology (http://ecco2.jpl.nasa.gov). DV and FL were supported by the
NASA Physical Oceanography program. SK was supported by the Russian
Federal Targeted program.
NR 33
TC 7
Z9 7
U1 1
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0278-4343
J9 CONT SHELF RES
JI Cont. Shelf Res.
PD SEP 1
PY 2013
VL 66
BP 92
EP 104
DI 10.1016/j.csr.2013.07.007
PG 13
WC Oceanography
SC Oceanography
GA 222IL
UT WOS:000324724300010
ER
PT J
AU Dong, ZX
Wejinya, UC
Chalamalasetty, SNS
Meyyappan, M
AF Dong, Zhuxin
Wejinya, Uchechukwu C.
Chalamalasetty, Siva Naga Sandeep
Meyyappan, M.
TI Dimensional Analysis and Mechanical Properties Characterization of
Carbon Nanofibers under Subzero Temperatures
SO IEEE TRANSACTIONS ON NANOTECHNOLOGY
LA English
DT Article
DE Atomic force microscopy (AFM); carbon nanofibers; mechanical properties;
nanoindentation; subzero
ID NANOELECTRODE ARRAYS; NANOTUBES; BIOSENSORS; ELECTRODE; STRENGTH; ACID
AB The ability of carbon nanofibers grown on nanoelectrode chips for ultrafast detection of molecules down to parts per billion (ppb) with a response time in seconds and with a minimal usage of power has attracted the attention of materials researchers and nanotechnology explorers-for example, space research organizations. Application in chemical and biological sensing is being studied extensively. NASA in their report on failure of space missions released in 2008 emphasized on the need for studying extreme environmental behavior of futuristic space materials. Very little work has been done to understand the behavior of the nanofibers operating in low-temperature environments. In this paper, vertically aligned carbon nanofibers (VACNFs) have been characterized for their survival in extreme low-temperature environments using a combination of environmental chamber and atomic force microscopy (AFM). Specifically, this paper characterizes through nanoindentation the mechanical properties and dimensional stability of VACNFs operating in low-temperature environments.
C1 [Dong, Zhuxin; Wejinya, Uchechukwu C.] Univ Arkansas, Dept Mech Engn, Fayetteville, AR 72701 USA.
[Chalamalasetty, Siva Naga Sandeep] Univ Arkansas, Microelect & Photon Grad Program, Fayetteville, AR 72701 USA.
[Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
RP Dong, ZX (reprint author), Univ Notre Dame, Dept Civil & Environm Engn & Earth Sci, Notre Dame, IN 46556 USA.
EM zdong1@nd.edu; uwejinya@uark.edu; schalama@uark.edu;
m.meyyappan@nasa.gov
FU University of Arkansas, College of Engineering External Mentoring Award
Program
FX Manuscript received January 8, 2012; revised January 17, 2013 and May
17, 2013; accepted July 19, 2013. Date of publication July 24, 2013;
date of current version September 4, 2013. This work was supported in
part by the University of Arkansas, College of Engineering External
Mentoring Award Program. The review of this paper was arranged by
Associate Editor L. Dong
NR 24
TC 0
Z9 0
U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1536-125X
J9 IEEE T NANOTECHNOL
JI IEEE Trans. Nanotechnol.
PD SEP
PY 2013
VL 12
IS 5
BP 810
EP 816
DI 10.1109/TNANO.2013.2274519
PG 7
WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology;
Materials Science, Multidisciplinary; Physics, Applied
SC Engineering; Science & Technology - Other Topics; Materials Science;
Physics
GA 219JH
UT WOS:000324501600022
ER
PT J
AU Vernier, JP
Fairlie, TD
Murray, JJ
Tupper, A
Trepte, C
Winker, D
Pelon, J
Garnier, A
Jumelet, J
Pavolonis, M
Omar, AH
Powell, KA
AF Vernier, J. -P.
Fairlie, T. D.
Murray, J. J.
Tupper, A.
Trepte, C.
Winker, D.
Pelon, J.
Garnier, A.
Jumelet, J.
Pavolonis, M.
Omar, A. H.
Powell, K. A.
TI An Advanced System to Monitor the 3D Structure of Diffuse Volcanic Ash
Clouds
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
DE Aerosols; Satellite observations; Transportation meteorology
ID DISPERSION MODEL; RETRIEVAL; AEROSOLS; LIDAR; IASI
AB Major disruptions of the aviation system from recent volcanic eruptions have intensified discussions about and increased the international consensus toward improving volcanic ash warnings. Central to making progress is to better discern low volcanic ash loadings and to describe the ash cloud structure more accurately in three-dimensional space and time. Here, dispersed volcanic ash observed by the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) space-based lidar near 20 000-40 000 ft [~(6-13) km] over Australia and New Zealand during June 2011 is studied. This ash event took place 3 weeks after the Puyehue-Cordon Caulle eruption, which disrupted air traffic in much of the Southern Hemisphere. The volcanic ash layers are shown to exhibit color ratios (1064/532 nm) near 0.5, significantly lower than unity, as is observed with ice. Those optical properties are used to develop an ash detection algorithm. A "trajectory mapping" technique is then demonstrated wherein ash cloud observations are ingested into a Lagrangian model and used to construct ash dispersion maps and cross sections. Comparisons of the model results with independent observations suggest that the model successfully reproduces the 3D structure of volcanic ash clouds. This technique has a potential operational application in providing important additional information to worldwide volcanic ash advisory centers.
C1 [Vernier, J. -P.; Garnier, A.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Vernier, J. -P.; Fairlie, T. D.; Murray, J. J.; Trepte, C.; Winker, D.; Garnier, A.; Omar, A. H.; Powell, K. A.] NASA Langley Res Ctr, Hampton, VA USA.
[Tupper, A.] Australian Bur Meteorol, Northern Terr Reg Off, Casuarina, NT, Australia.
[Pelon, J.; Jumelet, J.] Univ Paris 06, CNRS, Univ Versailles St Quentin, Lab Atmospheres,INSU, Paris, France.
[Pavolonis, M.] NOAA, Natl Environm Satellite Data & Informat Serv, Madison, WI USA.
RP Vernier, JP (reprint author), Sci Syst & Applicat Inc, 11 Langley Blvd, Hampton, VA 23666 USA.
EM jeanpaul.vernier@nasa.gov
RI Pavolonis, Mike/F-5618-2010; Omar, Ali/D-7102-2017
OI Pavolonis, Mike/0000-0001-5822-219X; Omar, Ali/0000-0003-1871-9235
NR 39
TC 10
Z9 10
U1 2
U2 31
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD SEP
PY 2013
VL 52
IS 9
BP 2125
EP 2138
DI 10.1175/JAMC-D-12-0279.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 217YP
UT WOS:000324399700013
ER
PT J
AU Rosario-Castro, BI
Contes-de Jesus, EJ
Lebron-Colon, M
Meador, MA
Gonzalez-Gonzalez, I
Cabrera, CR
AF Rosario-Castro, Belinda I.
Contes-de Jesus, Enid J.
Lebron-Colon, Marisabel
Meador, Michael A.
Gonzalez-Gonzalez, Ileana
Cabrera, Carlos R.
TI Electrochemical lithium intercalation at single-wall carbon nanotubes
chemically attached to 4-aminothiophenol modified platinum electrodes
SO JOURNAL OF ELECTROANALYTICAL CHEMISTRY
LA English
DT Article
DE 4-Aminothiophenol; Platinum electrodes; Lithium intercalation; Single
wall carbon nanotubes
ID ION BATTERIES; GRAPHITE ELECTRODE; ENERGY-STORAGE; SURFACE; LI; XPS;
DECOMPOSITION; GROWTH
AB The electrochemical intercalation of lithium has been studied by cyclic voltammetry experiments at single wall carbon nanotubes (SWCNTs) chemically attached at Pt electrodes with 4-aminothiophenol (4ATP). Cyclic voltammetric studies of Li+ at SWCNT/4ATP/Pt electrodes were done evaluate the reversibility of Li intercalation. High-resolution X-ray photoelectron spectroscopy, X-ray diffraction, scanning electron microscopy, and reflection-absorption infrared spectroscopy were done to characterize the structural changes of SWCNT5/4-ATP/Pt electrodes upon electrochemical lithium intercalation. The reversible energy capacity obtained from charge/discharge studies showed a change from 538 mAh/g at the first charge/discharge cycle to 703 mAh/g, at the fifth cycle. The calculated Li storage capacity for SWCNTs/4-ATP/Pt electrodes almost doubled the theoretical capacity for Li intercalation in graphite electrodes. (C) 2013 Published by Elsevier B.V.
C1 [Rosario-Castro, Belinda I.; Contes-de Jesus, Enid J.; Gonzalez-Gonzalez, Ileana; Cabrera, Carlos R.] Univ Puerto Rico, Dept Chem, San Juan, PR 00931 USA.
[Rosario-Castro, Belinda I.; Contes-de Jesus, Enid J.; Gonzalez-Gonzalez, Ileana; Cabrera, Carlos R.] Univ Puerto Rico, NASA URC Ctr Adv Nanoscale Mat, San Juan, PR 00931 USA.
[Lebron-Colon, Marisabel; Meador, Michael A.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Cabrera, CR (reprint author), Univ Puerto Rico, Dept Chem, Rio Piedras Campus,POB 23346, San Juan, PR 00931 USA.
EM carlos.cabrera2@upr.edu
OI Cabrera, Carlos/0000-0002-3342-8666
FU NASA-URC [NNX10AQ17A]; NSF-NSEC Center for Hierarchical Manufacturing
[CHM-CMMI-053117]; NASA Graduate Student Researcher Program (GSRP)
Fellowship [NGT3-52381]
FX The authors acknowledges the assistance of members of the Materials
Characterization Center and the NASA Center for Advanced Nanoscale
Materials, both at the University of Puerto Rico, Rio Piedras Campus.
This project was partially funded by NASA-URC Grant Number NNX10AQ17A
and NSF-NSEC Center for Hierarchical Manufacturing (CHM-CMMI-053117).
B.I.R.C. would like to acknowledge the financial support from NASA
Graduate Student Researcher Program (GSRP) Fellowship (NGT3-52381).
NR 38
TC 0
Z9 0
U1 1
U2 13
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 1572-6657
J9 J ELECTROANAL CHEM
JI J. Electroanal. Chem.
PD SEP 1
PY 2013
VL 704
BP 242
EP 248
DI 10.1016/j.jelechem.2013.06.011
PG 7
WC Chemistry, Analytical; Electrochemistry
SC Chemistry; Electrochemistry
GA 221KV
UT WOS:000324658700034
ER
PT J
AU Noell, AC
Greenwood, AR
Lee, CM
Ponce, A
AF Noell, Aaron C.
Greenwood, Arin R.
Lee, Christine M.
Ponce, Adrian
TI High-density, homogeneous endospore monolayer deposition on test
surfaces
SO JOURNAL OF MICROBIOLOGICAL METHODS
LA English
DT Article
DE B. subtilis; Spores; Vacuum filtration; Inactivation; Deposition
ID BACILLUS-SUBTILIS SPORES; ANTHRACIS; DECONTAMINATION; DIFFICILE; DROPS;
FLOW
AB Bacillus subtilis spores were deposited in high-density single layers on metal, glass, and polymer substrates using vacuum filtration followed by a wetted filter transfer step. Quantitative analysis of spore transfer was performed using culture-based and germinability assays, and spore distributions were observed with electron microscopy. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Noell, Aaron C.; Greenwood, Arin R.; Lee, Christine M.; Ponce, Adrian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ponce, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM adrian.ponce@jpl.nasa.gov
FU Amgen Scholars program; Department of Homeland Security; NASA
Postdoctoral Program; NASA Astrobiology Institute Icy Worlds team;
National Aeronautics and Space Administration
FX The Authors would like to acknowledge funding support from the Amgen
Scholars program, the Department of Homeland Security, the NASA
Postdoctoral Program, and the NASA Astrobiology Institute Icy Worlds
team. 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.
NR 23
TC 1
Z9 1
U1 1
U2 14
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-7012
J9 J MICROBIOL METH
JI J. Microbiol. Methods
PD SEP
PY 2013
VL 94
IS 3
BP 245
EP 248
DI 10.1016/j.mimet.2013.05.003
PG 4
WC Biochemical Research Methods; Microbiology
SC Biochemistry & Molecular Biology; Microbiology
GA 221NB
UT WOS:000324664500015
PM 23719028
ER
PT J
AU Chu, E
Goebel, DM
Wirz, RE
AF Chu, Emily
Goebel, Dan M.
Wirz, Richard E.
TI Reduction of Energetic Ion Production in Hollow Cathodes by External Gas
Injection
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
AB Studies of the hollow-cathode discharge have shown the existence of energetic ions at high-discharge currents that are likely responsible for the high erosion rates observed on the cathode keeper electrode. This work examines the effect of neutral gas injection in the discharge plume of a 250 A lanthanum hexaboride hollow cathode on the production of energetic ions to determine the conditions that yield cathode operation and life. Two different gas injector types are used to deliver neutral gas into the discharge plume and a retarding-potential analyzer is used for ion energy measurements. The flow splits between the cathode internal and external flows, and the number and locations of the external gas injection sites are examined as a function of the discharge current. It is found that increasing discharge current increases the energetic ion production at any given flow rate or injection location. External gas injection reduces energetic ion production for constant cathode flow, with collimated gas-jet injection performing better than distributed injection. Lifetime estimates of the keeper electrode surface due to sputter erosion by ion bombardment reveal that high-discharge current operation at low cathode gas flow produced very energetic ions and limited keeper lifetimes to less than 5000 h. Applying sufficient internal cathode gas flow and external gas injection can extend the keeper life to over 10,000 h at discharge currents of up to 200 A.
C1 [Chu, Emily] CALTECH, Jet Prop Lab, Elect Prop Grp, Jet Prop Lab Intern, Pasadena, CA 91109 USA.
[Goebel, Dan M.] CALTECH, Jet Prop Lab, Elect Prop Grp, Pasadena, CA 91109 USA.
[Wirz, Richard E.] Univ Calif Los Angeles, Mech & Aerosp Engn Dept, Los Angeles, CA 90024 USA.
RP Chu, E (reprint author), CALTECH, Jet Prop Lab, Elect Prop Grp, Jet Prop Lab Intern, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM emc2hu@gmail.com; dan.m.goebel@jpl.nasa.gov; wirz@ucla.edu
NR 25
TC 3
Z9 4
U1 0
U2 6
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
J9 J PROPUL POWER
JI J. Propul. Power
PD SEP-OCT
PY 2013
VL 29
IS 5
BP 1155
EP 1163
DI 10.2514/1.B34799
PG 9
WC Engineering, Aerospace
SC Engineering
GA 223FG
UT WOS:000324789500016
ER
PT J
AU Meyyappan, M
AF Meyyappan, M.
TI Nanostructured materials for supercapacitors
SO JOURNAL OF VACUUM SCIENCE & TECHNOLOGY A
LA English
DT Review
ID CARBON NANOTUBE ELECTRODES; DOUBLE-LAYER CAPACITORS;
CHEMICAL-VAPOR-DEPOSITION; HIGH-PERFORMANCE SUPERCAPACITOR;
GRAPHENE-BASED SUPERCAPACITOR; MULTILAYERED METAL-CATALYSTS; HIGH-POWER
SUPERCAPACITORS; ELECTROCHEMICAL CHARACTERIZATION; IONIC-LIQUID;
MICROWAVE PLASMA
AB Supercapacitor is an energy storage device that attempts to combine the high power density of a capacitor with the high energy density of a battery. Conventional supercapacitors use carbon based electrodes, mostly graphite. In recent years, alternatives such as carbon nanotubes, graphene, and other nanostructured materials have been considered to construct supercapacitor electrodes. This article reviews the progress in this area in addition to presenting a brief background on supercapacitors as energy storage medium and nanomaterials. (C) 2013 American Vacuum Society.
C1 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
FU U.S. Army AMRDEC [MIPR2DO80R2388]
FX The author thanks Cattien Nguyen, Darrell Niemann, and Bin Chen for many
valuable discussions. Partial support from U.S. Army AMRDEC
(MIPR2DO80R2388) was acknowledged.
NR 176
TC 12
Z9 12
U1 7
U2 321
PU A V S AMER INST PHYSICS
PI MELVILLE
PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA
SN 0734-2101
J9 J VAC SCI TECHNOL A
JI J. Vac. Sci. Technol. A
PD SEP
PY 2013
VL 31
IS 5
AR 050803
DI 10.1116/1.4802772
PG 14
WC Materials Science, Coatings & Films; Physics, Applied
SC Materials Science; Physics
GA 217UZ
UT WOS:000324388800004
ER
PT J
AU Ham, YG
Lim, M
Kug, JS
AF Ham, Yoo-Geun
Lim, Mijung
Kug, Jong-Seong
TI Importance of mean state in simulating different types of El Nino
revealed by SNU coupled GCMs
SO PROGRESS IN OCEANOGRAPHY
LA English
DT Review
ID OCEAN RECHARGE PARADIGM; PACIFIC RIM; WARM POOL; ENSO; CLIMATE; MODEL;
IMPACTS; EVENTS; PARAMETERIZATION; PRECIPITATION
AB Recent studies suggest that there are two types of El Nth events, which differ in terms of zonal distribution of sea-surface temperature (SST) anomalies. In this study, we investigate mechanisms in controlling simulation of two-types of El Nino using three different versions of the Seoul National University (SNU) air-sea coupled general circulation models.
The occurrences of two types of El Nino are related to the simulated climatological SST over the eastern Pacific. It is found that a model with relatively less canonical (or frequent Warm Pool or Central Pacific) El Nino occurrence has colder cold tongue in the equatorial central Pacific. Due to the cold mean SST and associated dryness over the eastern Pacific, positive El Nino-related SST anomalies over the eastern Pacific cannot trigger local convection effectively. The eastern Pacific dryness leads to the confinement of anomalous convective activity in the western Pacific, which results in weak canonical El Nino and reduction in canonical El Nino occurrence. Instead, the confined convective activity in the western Pacific can lead to strong SST anomalies over western-central Pacific through local air-sea interaction, which can increase Warm Pool (WP) El Nino occurrence. In addition, we found that mean equatorial thermocline structure is also related to the occurrences of WP El Nino and canonical El Nino that is, a model with deep thermocline depth simulates less WP El Nino occurrence, consistent with Yeh et al. (2009). (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Ham, Yoo-Geun] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Ham, Yoo-Geun] Morgan State Univ, Baltimore, MD 21239 USA.
[Lim, Mijung] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea.
[Kug, Jong-Seong] Korea Inst Ocean Sci & Technol, Ansan, South Korea.
RP Kug, JS (reprint author), Korea Inst Ocean Sci & Technol, Ansan, South Korea.
EM jskug@kiost.ac
RI KUG, JONG-SEONG/A-8053-2013
FU National Research Foundation of Korea; Korean Government (MEST)
[NRF-2009-C1AAA001-2009-0093]; KIOST [PE98915, PE98991]; Korea Institute
of Science and Technology Information [KSC-2012-C2-25]
FX This work was supported by the National Research Foundation of Korea
Grant Funded by Korean Government (MEST) (NRF-2009-C1AAA001-2009-0093)
and KIOST (PE98915, PE98991). The modeling integration was supported by
grant KSC-2012-C2-25 from Korea Institute of Science and Technology
Information.
NR 53
TC 1
Z9 1
U1 0
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0079-6611
J9 PROG OCEANOGR
JI Prog. Oceanogr.
PD SEP
PY 2013
VL 116
BP 130
EP 141
DI 10.1016/j.pocean.2013.07.005
PG 12
WC Oceanography
SC Oceanography
GA 218TO
UT WOS:000324455600008
ER
PT J
AU Zuber, MT
Smith, DE
Lehman, DH
Hoffman, TL
Asmar, SW
Watkins, MM
AF Zuber, Maria T.
Smith, David E.
Lehman, David H.
Hoffman, Tom L.
Asmar, Sami W.
Watkins, Michael M.
TI Gravity Recovery and Interior Laboratory (GRAIL): Mapping the Lunar
Interior from Crust to Core
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Gravity; Moon; Lunar; Remote sensing; Spacecraft
ID TRACKING DATA; FIELD; MOON; PROSPECTOR; CLEMENTINE; MISSION; MASCONS
AB The Gravity Recovery and Interior Laboratory (GRAIL) is a spacecraft-to-spacecraft tracking mission that was developed to map the structure of the lunar interior by producing a detailed map of the gravity field. The resulting model of the interior will be used to address outstanding questions regarding the Moon's thermal evolution, and will be applicable more generally to the evolution of all terrestrial planets. Each GRAIL orbiter contains a Lunar Gravity Ranging System instrument that conducts dual-one-way ranging measurements to measure precisely the relative motion between them, which in turn are used to develop the lunar gravity field map. Each orbiter also carries an Education/Public Outreach payload, Moon Knowledge Acquired by Middle-School Students (MoonKAM), in which middle school students target images of the Moon for subsequent classroom analysis. Subsequent to a successful launch on September 10, 2011, the twin GRAIL orbiters embarked on independent trajectories on a 3.5-month-long cruise to the Moon via the EL-1 Lagrange point. The spacecraft were inserted into polar orbits on December 31, 2011 and January 1, 2012. After a succession of 19 maneuvers the two orbiters settled into precision formation to begin science operations in March 1, 2012 with an average altitude of 55 km. The Primary Mission, which consisted of three 27.3-day mapping cycles, was successfully completed in June 2012. The extended mission will permit a second three-month mapping phase at an average altitude of 23 km. This paper provides an overview of the mission: science objectives and measurements, spacecraft and instruments, mission development and design, and data flow and data products.
C1 [Zuber, Maria T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Lehman, David H.; Hoffman, Tom L.; Asmar, Sami W.; Watkins, Michael M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Zuber, MT (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
EM zuber@mit.edu
FU NASA's Discovery Program; National Aeronautics and Space Administration
FX The GRAIL mission is supported by NASA's Discovery Program and is
performed under contract to the Massachusetts Institute of Technology.
Part of this work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 30
TC 36
Z9 36
U1 5
U2 27
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2013
VL 178
IS 1
BP 3
EP 24
DI 10.1007/s11214-012-9952-7
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 219ZM
UT WOS:000324550500002
ER
PT J
AU Asmar, SW
Konopliv, AS
Watkins, MM
Williams, JG
Park, RS
Kruizinga, G
Paik, M
Yuan, DN
Fahnestock, E
Strekalov, D
Harvey, N
Lu, WW
Kahan, D
Oudrhiri, K
Smith, DE
Zuber, MT
AF Asmar, Sami W.
Konopliv, Alexander S.
Watkins, Michael M.
Williams, James G.
Park, Ryan S.
Kruizinga, Gerhard
Paik, Meegyeong
Yuan, Dah-Ning
Fahnestock, Eugene
Strekalov, Dmitry
Harvey, Nate
Lu, Wenwen
Kahan, Daniel
Oudrhiri, Kamal
Smith, David E.
Zuber, Maria T.
TI The Scientific Measurement System of the Gravity Recovery and Interior
Laboratory (GRAIL) Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Gravity; Moon; Remote sensing; Spacecraft
ID TRACKING; FIELD; MODEL
AB The Gravity Recovery and Interior Laboratory (GRAIL) mission to the Moon utilized an integrated scientific measurement system comprised of flight, ground, mission, and data system elements in order to meet the end-to-end performance required to achieve its scientific objectives. Modeling and simulation efforts were carried out early in the mission that influenced and optimized the design, implementation, and testing of these elements. Because the two prime scientific observables, range between the two spacecraft and range rates between each spacecraft and ground stations, can be affected by the performance of any element of the mission, we treated every element as part of an extended science instrument, a science system. All simulations and modeling took into account the design and configuration of each element to compute the expected performance and error budgets. In the process, scientific requirements were converted to engineering specifications that became the primary drivers for development and testing. Extensive simulations demonstrated that the scientific objectives could in most cases be met with significant margin. Errors are grouped into dynamic or kinematic sources and the largest source of non-gravitational error comes from spacecraft thermal radiation. With all error models included, the baseline solution shows that estimation of the lunar gravity field is robust against both dynamic and kinematic errors and a nominal field of degree 300 or better could be achieved according to the scaled Kaula rule for the Moon. The core signature is more sensitive to modeling errors and can be recovered with a small margin.
C1 [Asmar, Sami W.; Konopliv, Alexander S.; Watkins, Michael M.; Williams, James G.; Park, Ryan S.; Kruizinga, Gerhard; Paik, Meegyeong; Yuan, Dah-Ning; Fahnestock, Eugene; Strekalov, Dmitry; Harvey, Nate; Lu, Wenwen; Kahan, Daniel; Oudrhiri, Kamal] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Asmar, SW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM sami.asmar@jpl.nasa.gov
FU NASA Discovery Program
FX The GRAIL mission is supported by the NASA Discovery Program under
contracts to the Massachusetts Institute of Technology and the Jet
Propulsion Laboratory. The work described in this paper was mostly
carried out at Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. The authors thank colleagues who have contributed to
this work or reviewed it, especially at JPL: Duncan McPherson, Ralph
Roncoli, William Folkner, Kevin Barltrop, Charles Dunn, William
Klipstein, Randy Dodge, William Bertch, Daniel Klein, Dong Shin, Stefan
Esterhausin, Slava Turyshev, Tom Hoffman, Charles Bell, Hoppy Price,
Neil Dahya, Joseph Beerer, Glen Havens, Robert Gounley, Ruth Fragoso,
Susan Kurtik, Behzad Raofi, and Dolan Highsmith. From Lockheed Martin
Space Systems Company (Denver): Stu Spath, Tim Linn, Ryan Olds, Dave
Eckart, and Brad Haack, Kevin Johnson, Carey Parish, Chris May, Rob
Chambers, Kristian Waldorff, Josh Wood, Piet Kallemeyn, Angus McMechan,
Cavan Cuddy, and Steve Odiorne. From the NASA Goddard Space Flight
Center: Frank Lemoine and David Rowlands, and from the University of
Texas: Byron Tapley and Srinivas Bettadpur.
NR 42
TC 11
Z9 12
U1 0
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 SEP
PY 2013
VL 178
IS 1
BP 25
EP 55
DI 10.1007/s11214-013-9962-0
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 219ZM
UT WOS:000324550500003
ER
PT J
AU Klipstein, WM
Arnold, BW
Enzer, DG
Ruiz, AA
Tien, JY
Wang, RT
Dunn, CE
AF Klipstein, William M.
Arnold, Bradford W.
Enzer, Daphna G.
Ruiz, Alberto A.
Tien, Jeffrey Y.
Wang, Rabi T.
Dunn, Charles E.
TI The Lunar Gravity Ranging System for the Gravity Recovery and Interior
Laboratory (GRAIL) Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE GRAIL; Gravity; Moon; GRACE; Ranging
AB The Lunar Gravity Ranging System (LGRS) flying on NASA's Gravity Recovery and Interior Laboratory (GRAIL) mission measures fluctuations in the separation between the two GRAIL orbiters with sensitivity below 0.6 microns/Hz(1/2). GRAIL adapts the mission design and instrumentation from the Gravity Recovery and Climate Experiment (GRACE) to a make a precise gravitational map of Earth's Moon. Phase measurements of Ka-band carrier signals transmitted between spacecraft with line-of-sight separations between 50 km to 225 km provide the primary observable. Measurements of time offsets between the orbiters, frequency calibrations, and precise orbit determination provided by the Global Positioning System on GRACE are replaced by an S-band time-transfer cross link and Deep Space Network Doppler tracking of an X-band radioscience beacon and the spacecraft telecommunications link. Lack of an atmosphere at the Moon allows use of a single-frequency link and elimination of the accelerometer compared to the GRACE instrumentation. This paper describes the implementation, testing and performance of the instrument complement flown on the two GRAIL orbiters.
C1 [Klipstein, William M.; Arnold, Bradford W.; Enzer, Daphna G.; Ruiz, Alberto A.; Tien, Jeffrey Y.; Wang, Rabi T.; Dunn, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Klipstein, WM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Klipstein@jpl.nasa.gov
FU NASA Discovery Program
FX The GRAIL mission is supported by the NASA Discovery Program under
contract to the Massachusetts Institute of Technology and the Jet
Propulsion Laboratory, California Institute of Technology. The research
described in this paper was carried out at JPL.
NR 6
TC 10
Z9 10
U1 1
U2 9
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2013
VL 178
IS 1
BP 57
EP 76
DI 10.1007/s11214-013-9973-x
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 219ZM
UT WOS:000324550500004
ER
PT J
AU Contreras, CS
Salama, F
AF Contreras, Cesar S.
Salama, Farid
TI LABORATORY INVESTIGATIONS OF POLYCYCLIC AROMATIC HYDROCARBON FORMATION
AND DESTRUCTION IN THE CIRCUMSTELLAR OUTFLOWS OF CARBON STARS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE astrochemistry; circumstellar matter; dust, extinction; ISM: molecules;
methods: laboratory; stars: carbon
ID ION-MOLECULE REACTIONS; PULSED DISCHARGE ENVIRONMENT; CAVITY RINGDOWN
SPECTROSCOPY; GAS-PHASE; INFRARED-SPECTROSCOPY; REACTION-MECHANISMS;
INTERSTELLAR-MEDIUM; DOWN SPECTROSCOPY; COMPLEX ORGANICS; BENZENE
AB The formation and destruction mechanisms of interstellar dust analogs formed from a variety of polycyclic aromatic hydrocarbon (PAH) and hydrocarbon molecular precursors are studied in the laboratory. We used the newly developed facility COSmIC, which simulates interstellar and circumstellar environments, to investigate both PAHs and species that include the cosmically abundant atoms O, N, and S. The species generated in a discharge plasma are detected, monitored, and characterized in situ using highly sensitive techniques that provide both spectral and ion mass information. We report here the first series of measurements obtained in these experiments which focus on the characterization of the most efficient molecular precursors in the chemical pathways that eventually lead to the formation of carbonaceous grains in the stellar envelopes of carbon stars. We compare and discuss the relative efficiencies of the various molecular precursors that lead to the formation of the building blocks of carbon grains. We discuss the most probable molecular precursors in terms of size and structure and the implications for the expected growth and destruction processes of interstellar carbonaceous dust.
C1 [Contreras, Cesar S.; Salama, Farid] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Contreras, Cesar S.] Bay Area Environm Res Inst, Sonoma, CA USA.
RP Contreras, CS (reprint author), NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM cesar.contreras@nasa.gov; Farid.Salama@nasa.gov
RI Salama, Farid/A-8787-2009
OI Salama, Farid/0000-0002-6064-4401
FU NASA SMD APRA Laboratory Astrophysics Program through the "Laboratory
Studies of Astrophysically Significant Carbon Molecules And Ions in
Support of Space Missions" grant; NASA SMD APRA Laboratory Astrophysics
Program through the "Carbon in the Galaxy's Consortium" grant; NPP
fellowship at NASA Ames
FX Support from the NASA SMD APRA Laboratory Astrophysics Program through
the "Laboratory Studies of Astrophysically Significant Carbon Molecules
And Ions in Support of Space Missions" and the "Carbon in the Galaxy's
Consortium" grants is gratefully acknowledged. C. Contreras held an NPP
fellowship at NASA Ames. The authors wish to acknowledge fruitful
discussions with L. Biennier, C. Ricketts, E. Sciamma-O'Brien, H.
Sabbah, R. Zare, and A. Tielens and the outstanding technical support of
R. Walker.
NR 85
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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 SEP
PY 2013
VL 208
IS 1
AR UNSP 6
DI 10.1088/0067-0049/208/1/6
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 214XS
UT WOS:000324172700006
ER
PT J
AU Newman, JA
Cooper, MC
Davis, M
Faber, SM
Coil, AL
Guhathakurta, P
Koo, DC
Phillips, AC
Conroy, C
Dutton, AA
Finkbeiner, DP
Gerke, BF
Rosario, DJ
Weiner, BJ
Willmer, CNA
Yan, RB
Harker, JJ
Kassin, SA
Konidaris, NP
Lai, K
Madgwick, DS
Noeske, KG
Wirth, GD
Connolly, AJ
Kaiser, N
Kirby, EN
Lemaux, BC
Lin, L
Lotz, JM
Luppino, GA
Marinoni, C
Matthews, DJ
Metevier, A
Schiavon, RP
AF Newman, Jeffrey A.
Cooper, Michael C.
Davis, Marc
Faber, S. M.
Coil, Alison L.
Guhathakurta, Puragra
Koo, David C.
Phillips, Andrew C.
Conroy, Charlie
Dutton, Aaron A.
Finkbeiner, Douglas P.
Gerke, Brian F.
Rosario, David J.
Weiner, Benjamin J.
Willmer, C. N. A.
Yan, Renbin
Harker, Justin J.
Kassin, Susan A.
Konidaris, N. P.
Lai, Kamson
Madgwick, Darren S.
Noeske, K. G.
Wirth, Gregory D.
Connolly, A. J.
Kaiser, N.
Kirby, Evan N.
Lemaux, Brian C.
Lin, Lihwai
Lotz, Jennifer M.
Luppino, G. A.
Marinoni, C.
Matthews, Daniel J.
Metevier, Anne
Schiavon, Ricardo P.
TI THE DEEP2 GALAXY REDSHIFT SURVEY: DESIGN, OBSERVATIONS, DATA REDUCTION,
AND REDSHIFTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmology: observations; galaxies: distances and redshifts; galaxies:
evolution; galaxies: fundamental parameters; galaxies: high-redshift;
galaxies: statistics; large-scale structure of universe; methods: data
analysis; surveys
ID SIMILAR-TO 1; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; ACTIVE GALACTIC
NUCLEI; GROTH STRIP SURVEY; EXTRAGALACTIC LEGACY SURVEY;
SPITZER-SPACE-TELESCOPE; OPTICAL-ROTATION CURVES; COLOR-DENSITY
RELATION; TULLY-FISHER RELATION
AB We describe the design and data analysis of the DEEP2 Galaxy Redshift Survey, the densest and largest high-precision redshift survey of galaxies at z similar to 1 completed to date. The survey was designed to conduct a comprehensive census of massive galaxies, their properties, environments, and large-scale structure down to absolute magnitude M-B = -20 at z similar to 1 via similar to 90 nights of observation on the Keck telescope. The survey covers an area of 2.8 deg(2) divided into four separate fields observed to a limiting apparent magnitude of R-AB = 24.1. Objects with z less than or similar to 0.7 are readily identifiable using BRI photometry and rejected in three of the four DEEP2 fields, allowing galaxies with z > 0.7 to be targeted similar to 2.5 times more efficiently than in a purely magnitude-limited sample. Approximately 60% of eligible targets are chosen for spectroscopy, yielding nearly 53,000 spectra and more than 38,000 reliable redshift measurements. Most of the targets that fail to yield secure redshifts are blue objects that lie beyond z similar to 1.45, where the [O II] 3727 angstrom doublet lies in the infrared. The DEIMOS 1200 line mm(-1) grating used for the survey delivers high spectral resolution (R similar to 6000), accurate and secure redshifts, and unique internal kinematic information. Extensive ancillary data are available in the DEEP2 fields, particularly in the Extended Groth Strip, which has evolved into one of the richest multiwavelength regions on the sky. This paper is intended as a handbook for users of the DEEP2 Data Release 4, which includes all DEEP2 spectra and redshifts, as well as for the DEEP2 DEIMOS data reduction pipelines. Extensive details are provided on object selection, mask design, biases in target selection and redshift measurements, the spec2d two-dimensional data-reduction pipeline, the spec1d automated redshift pipeline, and the zspec visual redshift verification process, along with examples of instrumental signatures or other artifacts that in some cases remain after data reduction. Redshift errors and catastrophic failure rates are assessed through more than 2000 objects with duplicate observations. Sky subtraction is essentially photon-limited even under bright OH sky lines; we describe the strategies that permitted this, based on high image stability, accurate wavelength solutions, and powerful B-spline modeling methods. We also investigate the impact of targets that appear to be single objects in ground-based targeting imaging but prove to be composite in Hubble Space Telescope data; they constitute several percent of targets at z similar to 1, approaching similar to 5%-10% at z > 1.5. Summary data are given that demonstrate the superiority of DEEP2 over other deep high-precision redshift surveys at z similar to 1 in terms of redshift accuracy, sample number density, and amount of spectral information. We also provide an overview of the scientific highlights of the DEEP2 survey thus far.
C1 [Newman, Jeffrey A.; Matthews, Daniel J.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Cooper, Michael C.] Univ Calif Irvine, Dept Phys & Astron, Ctr Galaxy Evolut, Irvine, CA 92697 USA.
[Davis, Marc; Madgwick, Darren S.] Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA.
[Faber, S. M.; Guhathakurta, Puragra; Koo, David C.; Phillips, Andrew C.; Conroy, Charlie; Harker, Justin J.; Lai, Kamson] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Coil, Alison L.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Conroy, Charlie; Finkbeiner, Douglas P.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dutton, Aaron A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Gerke, Brian F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Rosario, David J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Weiner, Benjamin J.; Willmer, C. N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Yan, Renbin] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA.
[Kassin, Susan A.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Kassin, Susan A.; Noeske, K. G.; Lotz, Jennifer M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Konidaris, N. P.; Kirby, Evan N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Wirth, Gregory D.] Keck Observ, Kamuela, HI 96743 USA.
[Connolly, A. J.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Kaiser, N.; Luppino, G. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Lemaux, Brian C.] Lab Astrophys Marseille, Marseilles, France.
[Lin, Lihwai] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Marinoni, C.] Ctr Phys Theor Marseilles, Marseilles, France.
[Metevier, Anne] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA.
[Schiavon, Ricardo P.] Liverpool John Moores Univ, Astrophys Res Inst, Wirral H41 1LD, Merseyside, England.
RP Newman, JA (reprint author), Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
EM janewman@pitt.edu; m.cooper@uci.edu; mdavis@berkeley.edu;
faber@ucolick.org; acoil@ucsd.edu; raja@ucolick.org; koo@ucolick.org;
phillips@ucolick.org; cconroy@cfa.harvard.edu; dutton@mpia.de;
dfinkbeiner@cfa.harvard.edu; bfgerke@lbl.gov; rosario@mpe.mpg.de;
bjw@as.arizona.edu; cnaw@as.arizona.edu; yanrenbin@gmail.com;
jharker@ucolick.org; susan.kassin@nasa.gov; npk@astro.caltech.edu;
klai@ucolick.org; noeske@stsci.edu; wirth@keck.hawaii.edu;
ajc@astro.washington.edu; kaiser@ifa.hawaii.edu; enk@astro.caltech.edu;
brian.lemaux@oamp.fr; lihwailin@asiaa.sinica.edu.tw; lotz@stsci.edu;
ger@ifa.hawaii.edu; marinoni@cpt.univ-mrs.fr; djm70@pitt.edu;
ajmetevier@gmail.com; R.P.Schiavon@ljmu.ac.uk
OI Weiner, Benjamin/0000-0001-6065-7483; Kirby, Evan/0000-0001-6196-5162
FU NSF Center for Particle Astrophysics; National Science Foundation [AST
95-29098, 00-711098, 05-07483, 08-08133, AST 00-71048, 05-07428,
08-07630, 08-06732, ARI 92-14621]; NASA [HST-AR-01947]; NASA through
Hubble Fellowship [51256.01, 51269.01, NAS 5-26555]; Space Telescope
Science Institute; CARA; Hubble Fellowships; Hubble Fellowship; Spitzer
Fellowship; W. M. Keck Foundation; University of California; NASA;
California Association for Research in Astronomy (Keck Observatory);
University of California/Lick Observatory
FX The DEEP2 survey was initiated under the auspices of the NSF Center for
Particle Astrophysics. Major grant support was provided by National
Science Foundation grants AST 95-29098, 00-711098, 05-07483, and
08-08133 to UCSC, AST 00-71048, 05-07428, and 08-07630 to UCB, and
08-06732 to the University of Pittsburgh. Computing hardware used to
analyze DEEP2 data was provided by Sun Microsystems. The HST ACS imaging
mosaic in EGS was constructed by Anton Koekemoer and Jennifer Lotz and
was funded by grant HST-AR-01947 from NASA. NASA imaging of the original
Groth Strip was planned and executed by Ed Groth and Jason Rhodes with
support from NAS5-1661 and NAG5-6279 to the WFPC1 IDT. Support for this
work was provided by NASA through Hubble Fellowship grants 51256.01 and
51269.01 awarded to E.N.K. and M.C.C., respectively, 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. Sandra Faber thank CARA for a generous research grant and
the Miller Institute at UC Berkeley for a Visiting Miller Professorship,
during which much of this paper was written. Jeffrey Newman and Alison
Coil acknowledge support from Hubble Fellowships during their DEEP2
work, and Michael Cooper acknowledges support from both Hubble and
Spitzer Fellowships.; Thanks are due to the many institutions and
individuals who have made the DEEP2 survey possible. First thanks go to
the W. M. Keck Foundation, the University of California, and NASA for
providing funds to construct and operate the Keck telescopes. Second, we
wish to thank the technical teams in the UCO/Lick Shops and at Keck
Observatory for their role in building and commissioning the DEIMOS
spectrograph and for their superb support during many observing runs.
Funds for the spectrograph were provided by instrumentation grant ARI
92-14621 from the National Science Foundation and instrument funds from
the California Association for Research in Astronomy (Keck Observatory)
and from the University of California/Lick Observatory.
NR 156
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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 SEP
PY 2013
VL 208
IS 1
AR UNSP 5
DI 10.1088/0067-0049/208/1/5
PG 57
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 214XS
UT WOS:000324172700005
ER
PT J
AU Wong, T
Hughes, A
Ott, J
Muller, E
Pineda, JL
Bernard, JP
Chu, YH
Fukui, Y
Gruendl, RA
Henkel, C
Kawamura, A
Klein, U
Looney, LW
Maddison, S
Mizuno, Y
Paradis, D
Seale, J
Welty, DE
AF Wong, Tony
Hughes, Annie
Ott, Juergen
Muller, Erik
Pineda, Jorge L.
Bernard, Jean-Philippe
Chu, You-Hua
Fukui, Yasuo
Gruendl, Robert A.
Henkel, Christian
Kawamura, Akiko
Klein, Ulrich
Looney, Leslie W.
Maddison, Sarah
Mizuno, Yoji
Paradis, Deborah
Seale, Jonathan
Welty, Daniel E.
TI THE MAGELLANIC MOPRA ASSESSMENT (MAGMA). I. THE MOLECULAR CLOUD
POPULATION OF THE LARGE MAGELLANIC CLOUD (vol 197, pg 16, 2011)
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Correction
C1 [Wong, Tony; Chu, You-Hua; Gruendl, Robert A.; Looney, Leslie W.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Hughes, Annie] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Ott, Juergen] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Muller, Erik; Kawamura, Akiko] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Pineda, Jorge L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bernard, Jean-Philippe; Paradis, Deborah] CNRS, IRAP, F-31028 Toulouse 4, France.
[Bernard, Jean-Philippe] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Fukui, Yasuo; Mizuno, Yoji] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Henkel, Christian] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Klein, Ulrich] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Maddison, Sarah] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Seale, Jonathan] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Welty, Daniel E.] Univ Chicago, Ctr Astron & Astrophys, Chicago, IL 60637 USA.
RP Wong, T (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
EM wongt@astro.illinois.edu
NR 3
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD SEP
PY 2013
VL 208
IS 1
AR UNSP 13
DI 10.1088/0067-0049/208/1/13
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 214XS
UT WOS:000324172700013
ER
PT J
AU Williams, DN
Bremer, T
Doutriaux, C
Patchett, J
Williams, S
Shipman, G
Miller, R
Pugmire, DR
Smith, B
Steed, C
Bethel, EW
Childs, H
Krishnan, H
Prabhat
Wehner, M
Silva, CT
Santos, E
Hoop, D
Ellqvist, T
Poco, J
Geveci, B
Chaudhary, A
Bauer, A
Pletzer, A
Kindig, D
Potter, GL
Maxwell, TP
AF Williams, Dean N.
Bremer, Timo
Doutriaux, Charles
Patchett, John
Williams, Sean
Shipman, Galen
Miller, Ross
Pugmire, David R.
Smith, Brian
Steed, Chad
Bethel, E. Wes
Childs, Hank
Krishnan, Harinarayan
Prabhat
Wehner, Michael
Silva, Claudio T.
Santos, Emanuele
Hoop, David
Ellqvist, Tommy
Poco, Jorge
Geveci, Berk
Chaudhary, Aashish
Bauer, Andy
Pletzer, Alexander
Kindig, Dave
Potter, Gerald L.
Maxwell, Thomas P.
CA Ultrascale Visualization Climate
TI Ultrascale Visualization of Climate Data
SO COMPUTER
LA English
DT Article
AB Collaboration across research, government, academic, and private sectors is integrating more than 70 scientific computing libraries and applications through a tailorable provenance framework, empowering scientists to exchange and examine data in novel ways.
C1 [Williams, Dean N.; Bremer, Timo; Doutriaux, Charles] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Patchett, John; Williams, Sean] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Shipman, Galen; Miller, Ross; Pugmire, David R.; Smith, Brian; Steed, Chad] Oak Ridge Natl Lab, Oak Ridge, TN USA.
[Bethel, E. Wes; Childs, Hank; Krishnan, Harinarayan; Prabhat; Wehner, Michael] Lawrence Berkeley Natl Lab, Berkeley, CA USA.
[Silva, Claudio T.; Santos, Emanuele; Hoop, David; Ellqvist, Tommy; Poco, Jorge] NYU, Polytech Inst, New York, NY 10003 USA.
[Potter, Gerald L.; Maxwell, Thomas P.] NASA, Goddard Space Flight Ctr, Washington, DC USA.
RP Williams, DN (reprint author), Lawrence Livermore Natl Lab, Livermore, CA USA.
EM williams13@llnl.gov; bremer5@llnl.gov; doutriaux1@llnl.gov;
patchett@lanl.gov; seanw@lanl.gov; gshipman@ornl.gov; rgmiller@ornl.gov;
pugmire@ornl.gov; smithbe@ornl.gov; steedca@ornl.gov; ewbethel@lbl.gov;
hchilds@lbl.gov; hkrishnan@lbl.gov; prabhat@lbl.gov; MFWehner@lbl.gov;
csilva@nyu.edu; emanuele@lia.ufc.br; dkoop@poly.edu;
tommy.ellqvist@yahoo.se; jpocom@nyu.edu; berk.geveci@kitware.com;
aashish.chaudhary@kitware.com; andy.bauer@kitware.com;
pletzer@txcorp.com; kindig@txcorp.com; gerald.potter@nasa.gov;
thomas.maxwell@nasa.gov
OI Steed, Chad/0000-0002-3501-909X; Poco, Jorge/0000-0001-9096-6287
FU Office of Science, Office of Biological and Environmental Research, of
the US Department of Energy [DE-AC02-05CH11231, DE-AC52-07NA27344];
National Aeronautics and Space Administration; DOE Office of Science
[DE-AC05-00OR22725]
FX This work is supported by the Director, Office of Science, Office of
Biological and Environmental Research, of the US Department of Energy,
under contracts DE-AC02-05CH11231 and DE-AC52-07NA27344 and by the
National Aeronautics and Space Administration. This research used
resources of the Oak Ridge Leadership Computing Facility at Oak Ridge
National Laboratory, which is supported by the DOE Office of Science
under Contract No. DE-AC05-00OR22725.
NR 6
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U2 27
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0018-9162
J9 COMPUTER
JI Computer
PD SEP
PY 2013
VL 46
IS 9
BP 68
EP 76
PG 9
WC Computer Science, Hardware & Architecture; Computer Science, Software
Engineering
SC Computer Science
GA 218UG
UT WOS:000324457400020
ER
PT J
AU Matsumoto, T
Tsuchiyama, A
Nakamura-Messenger, K
Nakano, T
Uesugi, K
Takeuchi, A
Zolensky, ME
AF Matsumoto, Toru
Tsuchiyama, Akira
Nakamura-Messenger, Keiko
Nakano, Tsukasa
Uesugi, Kentaro
Takeuchi, Akihisa
Zolensky, Michael E.
TI Three-dimensional observation and morphological analysis of organic
nanoglobules in a carbonaceous chondrite using X-ray micro-tomography
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID TAGISH LAKE; MINERALOGY; GRAINS; DUST; PARTICLES; METEORITE; NUCLEUS;
SAMPLES; OBJECT; ORIGIN
AB Organic nanoglobules are submicrometer spherical, often hollow organic grains ubiquitously distributed throughout primitive solar materials, such as carbonaceous chondrites. Until now, organic nanoglobules have been examined by TEM only after sectioning by ultramicrotomy so it has not been possible to determine whether fluids or mineral grains occur in the hollow cores. H2O-rich fluids might be present in hollows of the nanoglobules if they originate from dust particles composed of organic materials and ice prior to or in an early stage of the solar system formation or fluids incorporated into nanoglobules during aqueous alteration on the asteroidal parent body. In order to determine whether or not any fluids or mineral grains are present in the nanoglobules, a carbonaceous chondrite sample (Tagish Lake C2 meteorite) was observed non-destructively using synchrotron radiation-based X-ray CT (computed tomography), and then microtomed sections were observed using a transmission electron microscope (TEM). We observed three-dimensional shapes of thirty-eight organic nanoglobules in the meteorite sample. Their size and shape distributions are consistent with a hypothesis that nanoglobules originate from icy dust particles. Nanoglobule candidates observed in CT images were confirmed by the TEM images. However, the presence or absence of fluid could not be judged because CT images of nanoglobules are affected by X-ray refraction. Simulation of CT images by considering X-ray refraction shows that the presence or absence of water in nanoglobules cannot be distinguished with CT images alone. However the outer shapes of nanoglobules can be determined quantitatively and nanoglobules containing silicate cores can be easily identified. The thirty-eight nanoglobules we examined did not have silicate cores. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Matsumoto, Toru; Tsuchiyama, Akira] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Nakamura-Messenger, Keiko] ESC Jacobs Technol, Houston, TX 77058 USA.
[Nakamura-Messenger, Keiko; Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Nakano, Tsukasa] Geol Survey Japan, Natl Inst Adv Ind Sci & Technol, Tsukuba, Ibaraki 3058567, Japan.
[Uesugi, Kentaro; Takeuchi, Akihisa] SPring 8 Japan Synchrotron Radiat Res Inst, Sayo 6795198, Japan.
RP Matsumoto, T (reprint author), Osaka Univ, Dept Earth & Space Sci, 1-1 Machikaneyama Cho, Toyonaka, Osaka 5600043, Japan.
EM tmatsumoto@kueps.kyoto-u.ac.jp
FU Japan Ministry of Education, Culture, Sports, Science and Technology
[19104012]; NASA [NNH10ZDA001N]
FX We thank Jim Brook, Alan Hildebrand, Peter Brown and Charley Roots for
the pristine recovery of the Tagish Lake meteorite, and for permitting
its study. We also thank Dr. Scott Messenger for discussion. This paper
benefitted from helpful comments by Dr. Yabuta, an anonymous reviewer
and associate-editor Dr. Christian Koeberl. The tomography experiment
was performed under the approval of the SPring-8 Proposal Review
Committee (2009A1605). A. T. was supported by a Grant-in-aid of the
Japan Ministry of Education, Culture, Sports, Science and Technology
(19104012), and K. N.-M. by NASA Cosmochemistry grants NNH10ZDA001N.
NR 38
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U1 1
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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 SEP 1
PY 2013
VL 116
BP 84
EP 95
DI 10.1016/j.gca.2012.05.007
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 213DN
UT WOS:000324034600009
ER
PT J
AU Yueh, SH
Tang, WQ
Fore, AG
Neumann, G
Hayashi, A
Freedman, A
Chaubell, J
Lagerloef, GSE
AF Yueh, Simon H.
Tang, Wenqing
Fore, Alexander G.
Neumann, Gregory
Hayashi, Akiko
Freedman, Adam
Chaubell, Julian
Lagerloef, Gary S. E.
TI L-Band Passive and Active Microwave Geophysical Model Functions of Ocean
Surface Winds and Applications to Aquarius Retrieval
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article; Proceedings Paper
CT 12th Specialist Meeting on Microwave Radiometry and Remote Sensing
Applications
CY MAR 05-09, 2012
CL University of Rome, Frascati, ITALY
HO University of Rome
DE Microwave remote sensing; ocean wind; radar; radiometer
ID SEA-SURFACE; FIELD EXPERIMENTS; SALINITY; SCATTEROMETER; TEMPERATURE;
MISSION; EMISSIVITY; RADIOMETER; SPEED; WATER
AB The L-band passive and active microwave geophysical model functions (GMFs) of ocean surface winds from the Aquarius data are derived. The matchups of Aquarius data with the Special Sensor Microwave Imager (SSM/I) and National Centers for Environmental Prediction (NCEP) winds were performed and were binned as a function of wind speed and direction. The radar HH GMF is in good agreement with the PALSAR GMF. For wind speeds above 10 m.s(-1), the L-band ocean backscatter shows positive upwind-crosswind (UC) asymmetry; however, the UC asymmetry becomes negative between about 3 and 8 m.s(-1). The negative UC (NUC) asymmetry has not been observed in higher frequency (above C-band) GMFs for ASCAT or QuikSCAT. Unexpectedly, the NUC symmetry also appears in the L-band radiometer data. We find direction dependence in the Aquarius TBV, TBH, and third Stokes data with peak-to-peak modulations increasing from about a few tenths to 2 K in the range of 10-25-m.s(-1) wind speed. The validity of the GMFs is tested through application to wind and salinity retrieval from Aquarius data using the combined active-passive algorithm. Error assessment using the triple collocation analyses of SSM/I, NCEP, and Aquarius winds indicates that the retrieved Aquarius wind speed accuracy is excellent, with a random error of about 0.75 m.s(-1). The wind direction retrievals also appear reasonable and accurate above 10 m.s(-1). The results of the error analysis indicate that the uncertainty of the GMFs for the wind speed correction of vertically polarized brightness temperatures is about 0.14 K for wind speed up to 10 m.s(-1).
C1 [Yueh, Simon H.; Tang, Wenqing; Fore, Alexander G.; Neumann, Gregory; Hayashi, Akiko; Freedman, Adam; Chaubell, Julian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lagerloef, Gary S. E.] Earth & Space Res, Seattle, WA 98121 USA.
EM simon.yueh@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The work described in this paper was carried out by the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 34
TC 40
Z9 40
U1 0
U2 27
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 SEP
PY 2013
VL 51
IS 9
SI SI
BP 4619
EP 4632
DI 10.1109/TGRS.2013.2266915
PG 14
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 218LV
UT WOS:000324434900002
ER
PT J
AU Zheng, QH
Fok, MC
Zheng, YH
Lui, ATY
AF Zheng, Qiuhua
Fok, Mei-Ching
Zheng, Yihua
Lui, Anthony T. Y.
TI Non-linear whistler mode wave effects on magnetospheric energetic
electrons
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Nonlinear plasma wave; Energy transport; Pitch angle change
ID COHERENT VLF WAVES; PITCH-ANGLE; DIFFUSION-COEFFICIENTS; EMISSIONS;
FIELD
AB Electron energy transport due to nonlinear plasma-wave and particle interactions is carried out by waves and particles resonating with each other. Many previous nonlinear wave studies have only considered the main resonance between waves and electrons, since the contributions from other resonant orders were ignored as insignificant. We have found through test particle simulations, however, that although independent separate contributions from higher-order resonances can be small, they can have a rather significant impact on the main-order contribution and hence on the total nonlinear wave effects. Contributions from different orders can interfere with each other and the overall nonlinear wave effect is significantly different from that of just the major resonance. Therefore, in the nonlinear wave/particle interaction regime, contributions from different resonant orders are inseparable and contributions from higher order wave-particle resonances should all be included. Similarly, banded plasma waves should be used in nonlinear wave studies instead of assuming monochromatic waves. When the essential factors mentioned above are included, the overall electron transport due to the nonlinear plasma wave effects takes the form of a diffusion-like process, rather than advection, as reported in many previous studies. It is also found that electron transport induced by whistler mode waves is an important mechanism for the formation of the electron butterfly pitch-angle distribution. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Zheng, Qiuhua; Fok, Mei-Ching; Zheng, Yihua] NASA, Goddard Sci Flight Ctr, Heliophys Div, Greenbelt, MD 20770 USA.
[Zheng, Qiuhua] Univ Maryland, Dept Astron, College Pk, MD 20773 USA.
[Lui, Anthony T. Y.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Zheng, QH (reprint author), NASA, Goddard Sci Flight Ctr, Heliophys Div, 8800 Greenbelt Rd, Greenbelt, MD 20770 USA.
EM Qiuhua.Zheng@nasa.gov
RI Fok, Mei-Ching/D-1626-2012
FU NSF [ATM-0852508]
FX This work is supported by the NSF award ATM-0852508.
NR 34
TC 4
Z9 4
U1 0
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD SEP
PY 2013
VL 102
BP 8
EP 16
DI 10.1016/j.jastp.2013.03.018
PG 9
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 212WS
UT WOS:000324014100002
ER
PT J
AU Lee, JN
Wu, DL
Ruzmaikin, A
AF Lee, Jae N.
Wu, Dong L.
Ruzmaikin, Alexander
TI Interannual variations of MLS carbon monoxide induced by solar cycle
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Carbon monoxide; Total solar irradiance; Middle atmosphere; Microwave
Limb Sounder
ID II SOLSTICE-II; CROSS-SECTION MEASUREMENTS; IRRADIANCE MONITOR TIM;
MIDDLE ATMOSPHERE; TEMPERATURE-DEPENDENCE; SORCE MISSION; PROTON EVENTS;
CLIMATE; CO; SOUNDER
AB More than eight years (2004-2012) of carbon monoxide (CO) measurements from the Aura Microwave Limb Sounder (MLS) are analyzed. The mesospheric CO, largely produced by the carbon dioxide (CO2) photolysis in the lower thermosphere, is sensitive to the solar irradiance variability. The long-term variation of observed mesospheric MLS CO concentrations at high latitudes is likely driven by the solar-cycle modulated UV forcing. Despite of different CO abundances in the southern and northern hemispheric winter, the solar-cycle dependence appears to be similar. This solar signal is further carried down to the lower altitudes by the dynamical descent in the winter polar vortex. Aura MLS CO is compared with the Solar Radiation and Climate Experiment (SORCE) total solar irradiance (TSI) and also with the spectral irradiance in the far ultraviolet (FUV) region from the SORCE Solar-Stellar Irradiance Comparison Experiment (SOLSTICE). Significant positive correlation (up to 0.6) is found between CO and FUV/TSI in a large part of the upper atmosphere. The distribution of this positive correlation in the mesosphere is consistent with the expectation of CO changes induced by the solar irradiance variations. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Lee, Jae N.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Wu, Dong L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ruzmaikin, Alexander] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Lee, JN (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
EM jae.n.lee@nasa.gov
FU NASA Living With a Star Targeted Research and Technology Program
[NNH10ZDA001N-LWSTRT]
FX This work is supported by the NASA Living With a Star Targeted Research
and Technology Program (NNH10ZDA001N-LWSTRT). We thank the Aura MLS and
SORCE teams for providing their data and analysis support. We thank two
anonymous reviewers for valuable comments and suggestions that led to an
improved manuscript
NR 33
TC 3
Z9 3
U1 0
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD SEP
PY 2013
VL 102
BP 99
EP 104
DI 10.1016/j.jastp.2013.05.012
PG 6
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 212WS
UT WOS:000324014100012
ER
PT J
AU Habarulema, JB
McKinnell, LA
Buresova, D
Zhang, YL
Seemala, G
Ngwira, C
Chum, J
Opperman, B
AF Habarulema, John Bosco
McKinnell, Lee-Anne
Buresova, Dalia
Zhang, Yongliang
Seemala, Gopi
Ngwira, Chigomezyo
Chum, Jaroslav
Opperman, Ben
TI A comparative study of TEC response for the African equatorial and
mid-latitudes during storm conditions
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Magnetic storms; African equatorial and midlatitude TEC dynamics; TIDs
ID TRAVELING IONOSPHERIC DISTURBANCES; TOTAL ELECTRON-CONTENT; SEVERE
MAGNETIC STORM; LATITUDE IONOSPHERE; GEOMAGNETIC STORMS; GRAVITY-WAVES;
MID-LATITUDE; F-REGION; GPS DATA; SATELLITE
AB The solar wind effects on the Earth's environment are studied for their basic scientific values and crucial practical impacts on technological systems. This paper reports results of Total Electron Content (TEC) changes during two successive ionospheric storms of 7-12 November 2004 using GPS data derived from dual frequency receivers located at African equatorial and midlatitudes. In the geographic coordinate system, equatorial TEC variability is considered over Libreville (036 degrees N, 9.67 degrees E), Gabon and Mbarara (0.60 degrees S, 30.74 degrees E), Uganda. TEC over midlatitude stations Sutherland (32.38 degrees S, 20.81 degrees E) and Springbok (29.67 degrees S, 17.88 degrees E), South Africa are analysed. The analysis of the storm time ionospheric variability over South Africa was undertaken by comparing the critical frequency of the F2 layer (foF2) and the peak height of the F2 layer (hmF2) values obtained from Grahamstown (33.30 degrees S, 26.53 degrees E) and Madimbo (22.4 degrees S, 30.9 degrees E) ionosonde measurements. During the analysed storm period it is observed that GPS TEC for midlatitudes was depleted significantly with a corresponding depletion in foF2, due to the reduction in GUVI O/N-2 ratio as observed from its global maps. Over the equatorial latitudes, positive storm effects are more dominant especially during the storm main phase. Negative storm effects are observed over both mid and equatorial latitudes during the recovery phase. A shift in equatorial TEC enhancement (from one GPS station to another) is observed during magnetic storms and has been partially attributed to passage of Travelling Ionospheric Disturbances (TIDs). Magnetometer data over the International Real-time Magnetic Observatory Network (intermagnet) station, Addis Ababa, ME (9.03 degrees N, 38.77 degrees E) has been used to help with the explanation of possible causes of equatorial ionospheric TEC dynamics during the analysed magnetic storm period. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Habarulema, John Bosco; McKinnell, Lee-Anne; Opperman, Ben] South African Natl Space Agcy SANSA Space Sci, ZA-7200 Hermanus, South Africa.
[Habarulema, John Bosco; McKinnell, Lee-Anne] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa.
[Buresova, Dalia; Chum, Jaroslav] AS CR, Inst Atmospher Phys, Prague 14131 4, Czech Republic.
[Zhang, Yongliang] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Seemala, Gopi] Kyoto Univ, Res Inst Sustainable Humanosphere, Uji, Kyoto 6110011, Japan.
[Ngwira, Chigomezyo] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Ngwira, Chigomezyo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Habarulema, JB (reprint author), South African Natl Space Agcy SANSA Space Sci, POB 32, ZA-7200 Hermanus, South Africa.
EM jhabarulema@sansa.org.za
RI Chum, Jaroslav/G-9514-2014; Buresova, Dalia/G-4514-2014; Seemala,
Gopi/J-7050-2012; Zhang, Yongliang/C-2180-2016;
OI Chum, Jaroslav/0000-0002-0486-0679; Seemala, Gopi/0000-0002-3690-7873;
Zhang, Yongliang/0000-0003-4851-1662; Habarulema, John
Bosco/0000-0002-9716-7688
FU South African National Space Agency (SANSA); National Research
Foundation (NRF), South Africa; Grant Agency of the Czech Republic
[P209/11/1908]
FX J.B. Habarulema's research is supported by the South African National
Space Agency (SANSA) and National Research Foundation (NRF), South
Africa. Data for the O/N2 ratio was obtained from
http://guvi.jhuapl.edu. The GUVI data used here is provided through
support from the NASA MO&DA program. The GUVI instrument was designed
and built by the Aerospace Corporation and the Johns Hopkins University.
The Principal Investigator is Dr. Andrew B. Christensen and the Chief
Scientist and co-PI is Dr. Larry J. Paxton. The solar wind data was
downloaded from Coordinated Data Analysis website (CDA Web), hosted by
the NASA/GSFC Space Physics Data Facility. IGS/GPS data for equatorial
stations was downloaded from ftp://garner.ucsd.edu while the South
African GPS data was provided by the Chief Directorate: National
Geo-spatial information, South Africa. Dalia Buresova's contribution was
supported by Grant no. P209/11/1908 of the Grant Agency of the Czech
Republic.
NR 53
TC 15
Z9 15
U1 2
U2 17
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD SEP
PY 2013
VL 102
BP 105
EP 114
DI 10.1016/j.jastp.2013.05.008
PG 10
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 212WS
UT WOS:000324014100013
ER
PT J
AU Wendt, V
Wust, S
Mlynczak, MG
Russell, JM
Yee, JH
Bittner, M
AF Wendt, Verena
Wuest, Sabine
Mlynczak, Martin G.
Russell, James M., III
Yee, Jeng-Hwa
Bittner, Michael
TI Impact of atmospheric variability on validation of satellite-based
temperature measurements
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Coincidence; Mismatch error; Natural variability; Validation
AB Satellite validation is often based on straight forward comparison of satellite-based data with non-satellite based measurements. For functional reasons satellite and reference measurements do usually not correspond exactly in time and space. Dynamical effects in the atmosphere lead to temporal and spatial variability of atmospheric parameters (e.g. temperature). This causes considerable differences that do not necessarily hint to an incorrect satellite measurement, so called mistime and misdistance errors.
In this paper, the natural variability of the atmosphere is studied on scales effecting validation measurements. The approach is applied to temperature data from the ERA-40 reanalysis as well as to radiosonde (SIGMA-1) and satellite-based (SABER) measurements. Mistime and misdistance errors are quantified in dependence of geographic position, altitude, season and the temporal and spatial mismatch. The results allow a quantitative estimation of the impact of natural variability on validation analyses. In general, values lie in the range of a few Kelvin (e.g. up to 5 K for 500 km misdistance or 6 h mistime in the stratosphere), which indicates considerable effects on validation results. The determined results also point out regions in the atmosphere where the impact of natural variability is in general relatively high (e.g. the winter stratosphere in mid-latitudes) or rather low (e.g. the lower summer stratosphere). Altitudes, which are characterized systematically by only small mismatch errors, are indicated at about 10 and 25 km, respectively. These quiet layers are of special interest for validation activities. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Wendt, Verena] Umweltforsch Stn Schneefernerhaus, Zugspitze, Germany.
[Wendt, Verena; Wuest, Sabine; Bittner, Michael] German Remote Sensing Data Ctr, DLR, Oberpfaffenhofen, Germany.
[Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Russell, James M., III] Ctr Atmospher Sci, Hampton, VA USA.
[Yee, Jeng-Hwa] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Bittner, Michael] Univ Augsburg, Inst Phys, D-86159 Augsburg, Germany.
RP Wendt, V (reprint author), Umweltforsch Stn Schneefernerhaus, Zugspitze, Germany.
EM verena.wendt@dlr.de
FU German Federal Ministry for Economy and Technology [50 EE 0702]
FX This study is being carried out by the Environmental Research Station
'Schneefernerhaus' (UFS) and the German Aerospace Center (DLR) in close
cooperation. It is supported with funds from the German Federal Ministry
for Economy and Technology (50 EE 0702).
NR 15
TC 4
Z9 4
U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD SEP
PY 2013
VL 102
BP 252
EP 260
DI 10.1016/j.jastp.2013.05.022
PG 9
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 212WS
UT WOS:000324014100028
ER
PT J
AU Wu, MLC
Reale, O
Schubert, SD
AF Wu, Man-Li C.
Reale, Oreste
Schubert, Siegfried D.
TI A Characterization of African Easterly Waves on 2.5-6-Day and 6-9-Day
Time Scales
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Dynamics; Waves; atmospheric; Filtering techniques; Spectral analysis;
models; distribution
ID INTERACTIONS CAUSING PRECIPITATION; POTENTIAL VORTICITY GRADIENT;
TROPICAL ATLANTIC; 3-DIMENSIONAL STRUCTURE; WEST-AFRICA; PHASE III;
NORTHWEST AFRICA; HILBERT SPECTRUM; NORTHERN SUMMER; DRY YEARS
AB This study shows that the African easterly wave (AEW) activity over the African monsoon region and the northern tropical Atlantic can be divided in two distinct temporal bands with time scales of 2.5-6 and 6-9 days. The results are based on a two-dimensional ensemble empirical mode decomposition (2D-EEMD) of the Modern-Era Retrospective Analysis for Research and Applications (MERRA). The novel result of this investigation is that the 6-9-day waves appear to be located predominantly to the north of the African easterly jet (AEJ), originate at the jet level, and are different in scale and structure from the well-known low-level 2.5-6-day waves that develop baroclinically on the poleward flank of the AEJ. Moreover, they appear to interact with midlatitude eastward-propagating disturbances, with the strongest interaction taking place at the latitudes where the core of the Atlantic high pressure system is located. Composite analyses applied to the mode decomposition indicate that the interaction of the 6-9-day waves with midlatitude systems is characterized by enhanced southerly (northerly) flow from (toward) the tropics. This finding agrees with independent studies focused on European floods, which have noted enhanced moist transport from the ITCZ toward the Mediterranean region on time scales of about a week as important precursors of extreme precipitation.
C1 [Wu, Man-Li C.; Schubert, Siegfried D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Reale, Oreste] NASA, Goddard Space Flight Ctr, Earth Sci Div Atmospheres, Greenbelt, MD 20771 USA.
[Reale, Oreste] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
RP Reale, O (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Div Atmospheres, Code 610-8, Greenbelt, MD 20771 USA.
EM oreste.reale-1@nasa.gov
FU NASA Earth Science Enterprises Global Modeling and Analysis Program
FX This work was supported by the NASA Earth Science Enterprises Global
Modeling and Analysis Program. Thanks are due to anonymous reviewers for
helpful comments.
NR 62
TC 6
Z9 6
U1 2
U2 7
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 SEP
PY 2013
VL 26
IS 18
BP 6750
EP 6774
DI 10.1175/JCLI-D-12-00336.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 213LB
UT WOS:000324057600003
ER
PT J
AU Taylor, PC
Cai, M
Hu, AX
Meehl, J
Washington, W
Zhang, GJ
AF Taylor, Patrick C.
Cai, Ming
Hu, Aixue
Meehl, Jerry
Washington, Warren
Zhang, Guang J.
TI A Decomposition of Feedback Contributions to Polar Warming Amplification
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Climate change; Climate sensitivity; Feedback; Forcing
ID COMMUNITY ATMOSPHERE MODEL; GENERAL-CIRCULATION MODEL; GREENHOUSE-PLUS
FEEDBACK; CLIMATE MODEL; ARCTIC AMPLIFICATION; RADIATIVE-TRANSFER; CO2
CONCENTRATION; PART II; SENSITIVITY; FRAMEWORK
AB Polar surface temperatures are expected to warm 2-3 times faster than the global-mean surface temperature: a phenomenon referred to as polar warming amplification. Therefore, understanding the individual process contributions to the polar warming is critical to understanding global climate sensitivity. The Coupled Feedback Response Analysis Method (CFRAM) is applied to decompose the annual- and zonal-mean vertical temperature response within a transient 1% yr(-1) CO2 increase simulation of the NCAR Community Climate System Model, version 4 (CCSM4), into individual radiative and nonradiative climate feedback process contributions. The total transient annual-mean polar warming amplification (amplification factor) at the time of CO2 doubling is +2.12 (2.3) and +0.94 K (1.6) in the Northern and Southern Hemisphere, respectively. Surface albedo feedback is the largest contributor to the annual-mean polar warming amplification accounting for +1.82 and +1.04 K in the Northern and Southern Hemisphere, respectively. Net cloud feedback is found to be the second largest contributor to polar warming amplification (about +0.38 K in both hemispheres) and is driven by the enhanced downward longwave radiation to the surface resulting from increases in low polar water cloud. The external forcing and atmospheric dynamic transport also contribute positively to polar warming amplification: +0.29 and +0.32 K, respectively. Water vapor feedback contributes negatively to polar warming amplification because its induced surface warming is stronger in low latitudes. Ocean heat transport storage and surface turbulent flux feedbacks also contribute negatively to polar warming amplification. Ocean heat transport and storage terms play an important role in reducing the warming over the Southern Ocean and Northern Atlantic Ocean.
C1 [Taylor, Patrick C.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Cai, Ming] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Hu, Aixue; Meehl, Jerry; Washington, Warren] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Zhang, Guang J.] Univ Calif San Diego, Scripps Inst Oceanog, San Diego, CA 92103 USA.
RP Cai, M (reprint author), Florida State Univ, Dept Earth Ocean & Atmospher Sci, 1017 Acad Way, Tallahassee, FL 32306 USA.
EM mcai@fsu.edu
RI Hu, Aixue/E-1063-2013; Taylor, Patrick/D-8696-2015
OI Hu, Aixue/0000-0002-1337-287X; Taylor, Patrick/0000-0002-8098-8447
FU National Science Foundation [ATM-0833001, ATM-0832915]; NOAA CPO/CPPA
program [NA10OAR4310168]; DOE Office of Science Regional and Global
Climate Modeling (RGCM) program [DE-SC0004974]; Office of Science (BER),
U.S. Department of Energy [DE-FC02-97ER62402]; National Science
Foundation
FX This research was in part supported by research grants from the National
Science Foundation (ATM-0833001 and ATM-0832915), the NOAA CPO/CPPA
program (NA10OAR4310168), and DOE Office of Science Regional and Global
Climate Modeling (RGCM) program (DE-SC0004974). Portions of this study
were supported by the Office of Science (BER), U.S. Department of
Energy, Cooperative Agreement DE-FC02-97ER62402, and the National
Science Foundation.
NR 51
TC 44
Z9 44
U1 3
U2 42
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD SEP
PY 2013
VL 26
IS 18
BP 7023
EP 7043
DI 10.1175/JCLI-D-12-00696.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 213LB
UT WOS:000324057600016
ER
PT J
AU Rizvi, F
Weitl, RM
AF Rizvi, Farheen
Weitl, Raquel M.
TI Characterizing Limit Cycles in the Cassini Thrust Vector Control System
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
AB The Cassini spacecraft dynamics telemetry during long main engine burns has indicated the presence of stable limit cycles between 0.03 and 0.05 Hz frequencies. Even though these limit cycles have been observed in telemetry, they have not hindered the spacecraft performance to any degree of concern. The performance of the main engine thrust vector control system has been excellent throughout the prime and extended missions. However, it is important to understand these stable limit cycles from a controller design viewpoint. It is proposed that the observed limit cycles in the dynamics telemetry appear from a stable interaction between the unmodeled nonlinear elements and the linear main engine thrust vector control system. This paper focuses on one such nonlinearity that emerges from the gear backlash in the engine gimbal actuator system. The gear backlash nonlinearity is modeled via a describing function, and the interaction between the nonlinear element model and the overall dynamics of the spacecraft is studied. With this interaction, the stable limit cycle is reproduced analytically and in simulation. The results are compared with the actual telemetry from long burns like Saturn orbit insertion and main engine orbit trim maneuvers. The predicted stable limit cycle frequency and amplitude show good agreement within 6% error between the analytical, simulation, and telemetry results. This work claims that the stable limit cycles occur due to the stable interaction between the unmodeled nonlinear elements and linear main engine thrust vector control system.
C1 [Rizvi, Farheen] CALTECH, Jet Prop Lab, Guidance & Control Operat Grp, Guidance & Control Sect,Autonomous Syst Div, Pasadena, CA 91109 USA.
[Weitl, Raquel M.] CALTECH, Jet Prop Lab, End To End Informat Syst Grp, Syst Engn Sect,Syst & Software Div, Pasadena, CA 91109 USA.
RP Rizvi, F (reprint author), CALTECH, Jet Prop Lab, Guidance & Control Operat Grp, Guidance & Control Sect,Autonomous Syst Div, Mail Stop 230-104,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Farheen.Rizvi@jpl.nasa.gov; Raquel.M.Weitl@jpl.nasa.gov
NR 7
TC 1
Z9 1
U1 0
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD SEP-OCT
PY 2013
VL 36
IS 5
BP 1490
EP 1500
DI 10.2514/1.57295
PG 11
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 214SB
UT WOS:000324155000022
ER
PT J
AU Parker, JS
Anderson, RL
Peterson, A
AF Parker, Jeffrey S.
Anderson, Rodney L.
Peterson, Andrew
TI Surveying Ballistic Transfers to Low Lunar Orbit
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID HALO ORBITS; MOON; MISSION; EARTH; TRAJECTORIES
AB A simple strategy is identified to generate ballistic transfers between the Earth and Moon, i.e., transfers that perform two maneuvers: a translunar injection maneuver to depart the Earth and a lunar orbit insertion maneuver to insert into orbit at the Moon. This strategy is used to survey the performance of numerous transfers between varying Earth parking orbits and varying low lunar target orbits. The transfers surveyed include short three to six day direct transfers, longer three to four month low-energy transfers, and variants that include Earth phasing orbits and/or lunar flybys.
C1 [Parker, Jeffrey S.; Anderson, Rodney L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Peterson, Andrew] Georgia Inst Technol, Atlanta, GA 30332 USA.
RP Parker, JS (reprint author), CALTECH, Jet Prop Lab, M-S 301-121,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
OI Anderson, Rodney/0000-0001-5336-2775
NR 28
TC 5
Z9 5
U1 0
U2 5
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD SEP-OCT
PY 2013
VL 36
IS 5
BP 1501
EP 1511
DI 10.2514/1.55661
PG 11
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA 214SB
UT WOS:000324155000023
ER
PT J
AU Griffin, MJ
North, CE
Schulz, B
Amaral-Rogers, A
Bendo, G
Bock, J
Conversi, L
Conley, A
Dowell, CD
Ferlet, M
Glenn, J
Lim, T
Pearson, C
Pohlen, M
Sibthorpe, B
Spencer, L
Swinyard, B
Valtchanov, I
AF Griffin, M. J.
North, C. E.
Schulz, B.
Amaral-Rogers, A.
Bendo, G.
Bock, J.
Conversi, L.
Conley, A.
Dowell, C. D.
Ferlet, M.
Glenn, J.
Lim, T.
Pearson, C.
Pohlen, M.
Sibthorpe, B.
Spencer, L.
Swinyard, B.
Valtchanov, I.
TI Flux calibration of broad-band far-infrared and submillimetre
photometric instruments: theory and application to Herschel-SPIRE
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE instrumentation: photometers; methods: observational; techniques:
photometric; submillimetre: general
ID IN-FLIGHT; ABSOLUTE CALIBRATION; BOLOMETER CAMERA; PERFORMANCE;
TELESCOPE
AB Photometric instruments operating at far-infrared to millimetre wavelengths often have broad spectral passbands (lambda/delta lambda similar to 3 or less), especially those operating in space. A broad passband can result in significant variation of the beam profile and aperture efficiency across the passband, effects which thus far have not generally been taken into account in the flux calibration of such instruments. With absolute calibration uncertainties associated with the brightness of primary calibration standards now in the region of 5 per cent or less, variation of the beam properties across the passband can be a significant contributor to the overall calibration accuracy for extended emission. We present a calibration framework which takes such variations into account for both antenna-coupled and absorber-coupled focal plane architectures. The scheme covers point source and extended source cases, and also the intermediate case of a semi-extended source profile. We apply the new method to the Spectral and Photometric Imaging Receiver (SPIRE) photometer on board the Herschel Space Observatory.
C1 [Griffin, M. J.; North, C. E.; Amaral-Rogers, A.; Spencer, L.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Schulz, B.; Bock, J.] CALTECH, Pasadena, CA 91125 USA.
[Schulz, B.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Bendo, G.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Bock, J.; Dowell, C. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Conversi, L.; Valtchanov, I.] European Space Astron Ctr, ESA, Herschel Sci Ctr, E-28691 Madrid, Spain.
[Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Ferlet, M.; Lim, T.; Pearson, C.; Swinyard, B.] Rutherford Appleton Lab, Sci & Technol Facil Council, RAL Space, Didcot OX11 0QX, Oxon, England.
[Pearson, C.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Pohlen, M.] Gemini Observ Northern Operat Ctr, Hilo, HI 96720 USA.
[Sibthorpe, B.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands.
[Swinyard, B.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
RP Griffin, MJ (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
EM Matt.Griffin@astro.cf.ac.uk; chris.north@astro.cf.ac.uk
FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France);
ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA
(USA)
FX 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).
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DI 10.1093/mnras/stt999
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SC Astronomy & Astrophysics
GA 207XO
UT WOS:000323638200007
ER
PT J
AU Maestro, V
Che, X
Huber, D
Ireland, MJ
Monnier, JD
White, TR
Kok, Y
Robertson, JG
Schaefer, GH
Ten Brummelaar, TA
Tuthill, PG
AF Maestro, V.
Che, X.
Huber, D.
Ireland, M. J.
Monnier, J. D.
White, T. R.
Kok, Y.
Robertson, J. G.
Schaefer, G. H.
Ten Brummelaar, T. A.
Tuthill, P. G.
TI Optical interferometry of early-type stars with PAVO@CHARA - I.
Fundamental stellar properties
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: interferometric; stars: early-type; stars: fundamental
parameters
ID B-TYPE STARS; RAPIDLY ROTATING STARS; EFFECTIVE TEMPERATURES; ANGULAR
DIAMETERS; ATMOSPHERIC PARAMETERS; BOLOMETRIC CORRECTIONS; FLUX
CALIBRATION; MAIN-SEQUENCE; LINEAR RADII; O-ANDROMEDAE
AB We present interferometric observations of seven main-sequence and three giant stars with spectral types from B2 to F6 using the Precision Astronomical Visible Observations beam combiner at the Center for High Angular Resolution Astronomy array. We have directly determined the angular diameters for these objects with an average precision of 2.3 per cent. We have also computed bolometric fluxes using available photometry in the visible and infrared wavelengths, as well as space-based ultraviolet spectroscopy. Combined with precise Hipparcos parallaxes, we have derived a set of fundamental stellar properties including linear radius, luminosity and effective temperature. Fitting the latter to computed isochrone models, we have inferred masses and ages of the stars. The effective temperatures obtained are in good agreement (at a 3 per cent level) with nearly independent temperature estimations from spectroscopy. They validate recent sixth-order polynomial (B - V) - T-eff empirical relations, but suggest that a more conservative third-order solution could adequately describe the (V - K) - T-eff relation for main-sequence stars of spectral types A0 and later. Finally, we have compared mass values obtained combining surface gravity with inferred stellar radius (gravity mass) and as a result of the comparison of computed luminosity and temperature values with stellar evolutionary models (isochrone mass). The strong discrepancy between isochrone and gravity masses obtained for one of the observed stars, gamma Lyr, suggests that determination of the stellar atmosphere parameters should be revised.
C1 [Maestro, V.; Huber, D.; Ireland, M. J.; White, T. R.; Kok, Y.; Robertson, J. G.; Tuthill, P. G.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Che, X.; Monnier, J. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ireland, M. J.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Ireland, M. J.] Australian Astron Observ, N Ryde, NSW 1670, Australia.
[Schaefer, G. H.; Ten Brummelaar, T. A.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA.
RP Maestro, V (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
EM V.Maestro@physics.usyd.edu.au
FU NASA [NAS5-26555]; NASA Office of Space Science [NAG5-7584]; National
Aeronautics and Space Administration; National Science Foundation
[AST-0606958]; Georgia State University through the College of Arts and
Sciences; W. M. Keck Foundation; Australian Research Council
FX The authors would like to thank Chris Farrington, P.J. Goldfinger, Judit
Sturrman and Jo Cheng for their support during observations at the CHARA
array. This research has made use of the SIMBAD data base and the VizieR
catalogue access tool, operated at CDS, Strasbourg, France. Some 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-HST data is provided
by the NASA Office of Space Science via grant NAG5-7584 and by other
grants and contracts. This publication makes use of data products from
the Two Micron All Sky Survey, 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. The CHARA array is funded by the National Science Foundation
through NSF grant AST-0606958, by Georgia State University through the
College of Arts and Sciences and by the W. M. Keck Foundation. We
acknowledge the support of the Australian Research Council. VM is
supported by an International Denison Postgraduate Award. D. H. is
supported by an appointment to the NASA Postdoctoral Program at Ames
Research Center, administered by Oak Ridge Associated Universities
through a contract with NASA.
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EI 1365-2966
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JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2013
VL 434
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BP 1321
EP 1331
DI 10.1093/mnras/stt1092
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 207XO
UT WOS:000323638200028
ER
PT J
AU Levin, L
Bailes, M
Barsdell, BR
Bates, SD
Bhat, NDR
Burgay, M
Burke-Spolaor, S
Champion, DJ
Coster, P
D'Amico, N
Jameson, A
Johnston, S
Keith, MJ
Kramer, M
Milia, S
Ng, C
Possenti, A
Stappers, B
Thornton, D
van Straten, W
AF Levin, L.
Bailes, M.
Barsdell, B. R.
Bates, S. D.
Bhat, N. D. R.
Burgay, M.
Burke-Spolaor, S.
Champion, D. J.
Coster, P.
D'Amico, N.
Jameson, A.
Johnston, S.
Keith, M. J.
Kramer, M.
Milia, S.
Ng, C.
Possenti, A.
Stappers, B.
Thornton, D.
van Straten, W.
TI The High Time Resolution Universe Pulsar Survey -VIII. The Galactic
millisecond pulsar population
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: neutron; pulsars: general
ID DATA-ANALYSIS SYSTEMS; RADIO PULSARS; NEUTRON-STARS; RECYCLED PULSARS;
BINARY PULSARS; IONIZED-GAS; MILKY-WAY; DISCOVERY; LUMINOSITY; EVOLUTION
AB We have used millisecond pulsars (MSPs) from the southern High Time Resolution Universe (HTRU) intermediate latitude survey area to simulate the distribution and total population of MSPs in the Galaxy. Our model makes use of the scalefactor method, which estimates the ratio of the total number of MSPs in the Galaxy to the known sample. Using our best-fitting value for the z-height, z = 500 pc, we find an underlying population of MSPs of 8.3(+/- 4.2) x 10(4) sources down to a limiting luminosity of L-min = 0.1 mJy kpc(2) and a luminosity distribution with a steep slope of d log N/d log L = -1.45 +/- 0.14. However, at the low end of the luminosity distribution, the uncertainties introduced by small number statistics are large. By omitting very low luminosity pulsars, we find a Galactic population above L-min = 0.2 mJy kpc(2) of only 3.0(+/- 0.7) x 10(4) MSPs. We have also simulated pulsars with periods shorter than any known MSP, and estimate the maximum number of sub-MSPs in the Galaxy to be 7.8(+/- 5.0) x 10(4) pulsars at L = 0.1 mJy kpc(2). In addition, we estimate that the high and low latitude parts of the southern HTRU survey will detect 68 and 42 MSPs, respectively, including 78 new discoveries. Pulsar luminosity, and hence flux density, is an important input parameter in the model. Some of the published flux densities for the pulsars in our sample do not agree with the observed flux densities from our data set, and we have instead calculated average luminosities from archival data from the Parkes Telescope. We found many luminosities to be very different than their catalogue values, leading to very different population estimates. Large variations in flux density highlight the importance of including scintillation effects in MSP population studies.
C1 [Levin, L.; Bailes, M.; Barsdell, B. R.; Coster, P.; Jameson, A.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Levin, L.; Coster, P.; Johnston, S.; Keith, M. J.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Levin, L.; Bailes, M.; Barsdell, B. R.; Bhat, N. D. R.; Jameson, A.; van Straten, W.] Swinburne Univ Technol, ARC Ctr Excellence All Sky Astron CAASTRO, Hawthorn, Vic 3122, Australia.
[Levin, L.; Bates, S. D.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
[Bhat, N. D. R.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia.
[Burgay, M.; D'Amico, N.; Milia, S.; Possenti, A.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Italy.
[Burke-Spolaor, S.] NASA, Jet Prop Lab, Pasadena, CA 91106 USA.
[Champion, D. J.; Kramer, M.; Ng, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[D'Amico, N.; Milia, S.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy.
[Kramer, M.; Stappers, B.; Thornton, D.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
RP Levin, L (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Mail H30,POB 218, Hawthorn, Vic 3122, Australia.
EM lina.s.levin@gmail.com
OI Champion, David/0000-0003-1361-7723; Burgay, Marta/0000-0002-8265-4344;
van Straten, Willem/0000-0003-2519-7375
FU ARC Centre of Excellence for All-sky Astrophysics (CAASTRO);
Commonwealth of Australia
FX The work presented in this paper was conducted as part of L. Levin's PhD
thesis at Swinburne University and was originally written as a thesis
chapter. The version presented here has been slightly modified. This
work is supported by the ARC Centre of Excellence for All-sky
Astrophysics (CAASTRO). 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. This paper includes
archived data obtained through the Australia Telescope Online Archive
and the CSIRO Data Access Portal (http://data.csiro.au). The authors
would like to thank the referee for helpful comments and suggestions.
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JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2013
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BP 1387
EP 1397
DI 10.1093/mnras/stt1103
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 207XO
UT WOS:000323638200034
ER
PT J
AU van Putten, T
Watts, AL
D'Angelo, CR
Baring, MG
Kouveliotou, C
AF van Putten, T.
Watts, A. L.
D'Angelo, C. R.
Baring, M. G.
Kouveliotou, C.
TI Models of hydrostatic magnetar atmospheres at high luminosities
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: atmospheres; stars: magnetars; X-rays: bursts
ID PHOTOSPHERIC RADIUS EXPANSION; SOFT GAMMA-REPEATERS; X-RAY-BURSTS;
NEUTRON-STARS; GIANT FLARE; RADIATIVE MECHANISM; VACUUM POLARIZATION;
SPECTRA; SGR-1806-20; SGR-1900+14
AB We investigate the possibility of Photospheric Radius Expansion (PRE) during magnetar bursts. Identification of PRE would enable a determination of the magnetic Eddington limit (which depends on field strength and neutron star mass and radius), and shed light on the burst mechanism. To do this we model hydrostatic atmospheres in a strong radial magnetic field, determining both their maximum extent and their photospheric temperatures. We find that spatially extended atmospheres cannot exist in such a field configuration: typical maximum extent for magnetar-strength fields is similar to 10 m (as compared to 200 km in the non-magnetic case). Achieving balance of gravitational and radiative forces over a large range of radii, which is critical to the existence of extended atmospheres, is rendered impossible in strong fields due to the dependence of opacities on temperature and field strength. We conclude that high-luminosity bursts in magnetars do not lead to expansion and cooling of the photosphere, as in the non-magnetic case. We also find the maximum luminosity that can propagate through a hydrostatic magnetar atmosphere to be lower than previous estimates. The proximity and small extent of the photospheres associated with the two different polarization modes also call into question the interpretation of two blackbody fits to magnetar burst spectra as being due to extended photospheres.
C1 [van Putten, T.; Watts, A. L.; D'Angelo, C. R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
RP van Putten, T (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands.
EM T.vanPutten@uva.nl
FU ERC [247295]; NWO Vidi grant; NASA [NNX10AC59A, NNH07ZDA001-GLAST]
FX The authors would like to thank Cole Miller, Wynn Ho, Stuart Sim and
Ralph Wijers for useful discussions. TvP acknowledges support from the
ERC through Advanced Grant no. 247295. ALW and CD'A acknowledge support
from an NWO Vidi grant (PI Anna Watts). MGB thanks the NASA Astrophysics
Theory Program for support through grant NNX10AC59A. CK is partially
supported by NASA grant NNH07ZDA001-GLAST.
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BP 1398
EP 1410
DI 10.1093/mnras/stt1093
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 207XO
UT WOS:000323638200035
ER
PT J
AU Sutton, AD
Roberts, TP
Gladstone, JC
Farrell, SA
Reilly, E
Goad, MR
Gehrels, N
AF Sutton, Andrew D.
Roberts, Timothy P.
Gladstone, Jeanette C.
Farrell, Sean A.
Reilly, Emma
Goad, Michael R.
Gehrels, Neil
TI A bright ultraluminous X-ray source in NGC 5907
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion; accretion discs; black hole physics; X rays: binaries; X
rays: galaxies
ID HOLMBERG-II X-1; SPECTRAL STATE TRANSITIONS; MASS BLACK-HOLES; ESO
243-49; ACCRETION FLOWS; IX X-1; VARIABILITY; EVOLUTION; GALAXIES; HLX-1
AB We present a multimission X-ray analysis of a bright (peak observed 0.3-10 keV luminosity of similar to 6 x 10(40) erg s(-1)), but relatively highly absorbed ultraluminous X-ray source (ULX) in the edge-on spiral galaxy NGC 5907. The ULX is spectrally hard in X-rays (Gamma similar to 1.2-1.7, when fitted with an absorbed power law), and has a previously reported hard spectral break consistent with it being in the ultraluminous accretion state. It is also relatively highly absorbed for a ULX, with a column of similar to 0.4-0.9 x 10(22) atom cm(-2) in addition to the line-of-sight column in our Galaxy. Although its X-ray spectra are well represented by accretion disc models, its variability characteristics argue against this interpretation. The ULX spectra instead appear dominated by a cool, optically thick Comptonizing corona. We discuss how the measured 9 per cent rms variability and a hardening of the spectrum as its flux diminishes might be reconciled with the effects of a very massive, radiatively driven wind and subtle changes in the corona, respectively. We speculate that the cool disc-like spectral component thought to be produced by the wind in other ULXs may be missing from the observed spectrum due to a combination of a low temperature (similar to 0.1 keV), and the high column to the ULX. We find no evidence, other than its extreme X-ray luminosity, for the presence of an intermediate mass black hole (MsBHs, similar to 10(2)-10(4) M) in this object. Rather, the observations can be consistently explained by a massive ( 20 M) stellar remnant black hole in a super-Eddington accretion state.
C1 [Sutton, Andrew D.; Roberts, Timothy P.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Gladstone, Jeanette C.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Farrell, Sean A.; Reilly, Emma; Goad, Michael R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Farrell, Sean A.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Reilly, Emma] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sutton, AD (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England.
EM andrew.sutton@durham.ac.uk
FU UK Science and Technology Facilities Council; Avadh Bhatia Fellowship;
Alberta Ingenuity; ARC; University of Leicester; ESA Member States;
NASA; [DP110102889]
FX We thank the anonymous referee for their useful comments, that helped to
improve this paper. ADS gratefully acknowledges funding from the UK
Science and Technology Facilities Council in the form of a PhD
studentship, SAF for a postdoctoral position and TPR in the form of a
standard grant. JCG thanks the Avadh Bhatia Fellowship and Alberta
Ingenuity. SAF is also the recipient of an ARC Postdoctoral Fellowship,
funded by grant DP110102889. ER acknowledges the support of a Science
Undergraduate Research Experience scholarship from the University of
Leicester. This work is based on observations obtainedwithXMM-Newton, an
ESA science mission with instruments and contributions directly funded
by ESA Member States and NASA; the Chandra X-ray observatory; the Swift
Gamma Ray Burst Explorer; and ROSAT. It has also included observations
made with the NASA/ESA HST, and obtained from the HLA, which is a
collaboration between the Space Telescope Science Institute (STScI/NASA)
and the Canadian Astronomy Data Centre (CADC/NRC/CSA).
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DI 10.1093/mnras/stt1133
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SC Astronomy & Astrophysics
GA 207XO
UT WOS:000323638200061
ER
PT J
AU Heldmann, JL
Pollard, W
McKay, CP
Marinova, MM
Davila, A
Williams, KE
Lacelle, D
Andersen, DT
AF Heldmann, J. L.
Pollard, W.
McKay, C. P.
Marinova, M. M.
Davila, A.
Williams, K. E.
Lacelle, D.
Andersen, D. T.
TI The high elevation Dry Valleys in Antarctica as analog sites for
subsurface ice on Mars
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Ice; Mars; Polar regions; Antarctica; Drilling
ID SOUTHERN VICTORIA LAND; ROCK TEMPERATURE DATA; MIOCENE GLACIER ICE;
BEACON VALLEY; GROUND ICE; LOW RATES; SUBLIMATION; PERMAFROST;
STABILITY; SURFACE
AB The high elevation valleys of the McMurdo Dry Valleys of Antarctica are the only locations on Earth known to contain dry permafrost. The Dry Valleys are a hyper-arid polar desert environment and above 1500 m elevation, air temperatures do not exceed 0 degrees C and thus, similarly to Mars, liquid water is largely absent and instead the hydrologic cycle is dominated by frozen ice and vapor phase processes such as sublimation. These conditions make the high elevation Dry Valleys a key Mars analog location where periglacial processes and geomorphic features, and their use as a diagnostic for subsurface ice, can be studied in situ. Two valleys in the upper Dry Valleys show a diversity of subsurface ice; University Valley is dominated by dry permafrost overlying ice-cemented to ice-bonded ground and nearby middle Beacon Valley is dominated by massive ground ice. In both cases the ice is 10-60 cm below the surface. Here we compare the surface features in these two valleys to assess any correlation with the nature of the subsurface ice and compare these features to similar features seen at the Phoenix landing site on Mars. We conclude that while surface features may be indicative of ground ice, no specific correlations are possible and more direct methods are required to determine the nature of subsurface ice on Mars. (C) 2013 Published by Elsevier Ltd.
C1 [Heldmann, J. L.; McKay, C. P.; Marinova, M. M.; Davila, A.; Williams, K. E.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Pollard, W.] McGill Univ, Dept Geog, Montreal, PQ H3A 2T5, Canada.
[Marinova, M. M.] BAER Inst, West Sonoma, CA 95476 USA.
[Davila, A.; Andersen, D. T.] SETI Inst, Mountain View, CA 94041 USA.
[Williams, K. E.] Montana State Univ, Dept Earth Sci, Bozeman, MT 59717 USA.
[Lacelle, D.] Univ Ottawa, Dept Geog, Ottawa, ON K1N 6N5, Canada.
RP Heldmann, JL (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
EM Jennifer.Heldmann@nasa.gov
RI Davila, Alfonso/A-2198-2013;
OI Davila, Alfonso/0000-0002-0977-9909; Lacelle, Denis/0000-0002-6691-8717
FU NASA ASTEP program; NSF Office of Polar Programs; US Antarctic Program
FX This fieldwork was supported by the NASA ASTEP program, in collaboration
with the NSF Office of Polar Programs and the US Antarctic Program. We
acknowledge Brad Herried and the Antarctic Geospatial Information Center
(AGIC) for help with Antarctic mapping. Satellite imagery copyright
DigitalGlobe, Inc. and provided by NGA Commercial Imagery Program.
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SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP 1
PY 2013
VL 85
BP 53
EP 58
DI 10.1016/j.pss.2013.05.019
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 217MR
UT WOS:000324364100005
ER
PT J
AU Le Maistre, S
Rosenblatt, P
Rambaux, N
Castillo-Rogez, JC
Dehant, V
Marty, JC
AF Le Maistre, Sebastien
Rosenblatt, Pascal
Rambaux, Nicolas
Castillo-Rogez, Julie C.
Dehant, Veronique
Marty, Jean-Charles
TI Phobos interior from librations determination using Doppler and star
tracker measurements
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Rotation; Lander; Interior; Libration; Phobos; Doppler; Star tracker;
Tidal deformation
ID MARTIAN SATELLITES; GRAVITY-FIELD; SOLAR-SYSTEM; EVOLUTION; ORBITS;
MASSES; MODEL; MARS
AB Numerical simulations have been performed to assess the precision that can be obtained on Phobos libration angles by using two types of data acquired by a probe landed on the Martian moon: (1) Direct-To-Earth (DTE) Doppler data and (2) Star-Tracker (ST) data. Compared to independent estimates, combination of DTE and ST data provides the more precise estimates of Phobos libration angles at the 10(-3)-10(-5) degree level. Short period libration amplitudes are functions of the relative moments of inertia. Thus their determination would provide constraints on mass distributions inside Phobos. We show that the longitudinal libration amplitude at the orbital period, while being clearly distinct from the resonance period, is the most interesting signal for that purpose, because it leads to the best precision on (B-A)/C (10(-5) after only 10 weeks of operation). Nevertheless, we showed that inferring the individual moments of inertia A, B and C with a precision sufficient (<1%) to distinguish the rotational behavior of an homogenous from that of an heterogenous body requires the determination of one of the degree-two gravity field coefficient at the percent level.
In addition, we stress that ST and DTE data combination allows de-correlating librational motion from orbital motion since ST measurements are sensitive to the moon's rotation and do not depend on its ephemeris, whereas DTE Doppler data are sensitive to both motions as well as to Phobos' surface displacement due to the tides raised by Mars. Furthermore, the ephemeris of Phobos has to be known at the centimeter level to allow measuring the tidal surface displacement with enough precision to conclude on the nature of Phobos' interior (rubble pile versus monolithic) as one step toward constraining its origin and evolution. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Le Maistre, Sebastien; Rosenblatt, Pascal; Dehant, Veronique] Royal Observ Belgium, B-1180 Brussels, Belgium.
[Rambaux, Nicolas] Observ Paris, IMCCE, F-75014 Paris, France.
[Castillo-Rogez, Julie C.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Marty, Jean-Charles] Ctr Natl Etud Spatiales, F-31401 Toulouse, France.
RP Le Maistre, S (reprint author), Royal Observ Belgium, Av Circulaire 3, B-1180 Brussels, Belgium.
EM sebastien.lemaistre@oma.be
FU Belgian PRODEX program
FX This work was financially supported by the Belgian PRODEX program
managed by the European Space Agency in collaboration with the Belgian
Federal Science Policy Office. Part of this work was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under
Contract to NASA.
NR 37
TC 7
Z9 7
U1 0
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP 1
PY 2013
VL 85
BP 106
EP 122
DI 10.1016/j.pss.2013.06.015
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 217MR
UT WOS:000324364100009
ER
PT J
AU Schroder, SE
Mottola, S
Keller, HU
Raymond, CA
Russell, CT
AF Schroeder, S. E.
Mottola, S.
Keller, H. U.
Raymond, C. A.
Russell, C. T.
TI Resolved photometry of Vesta reveals physical properties of crater
regolith
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Vesta; Photometry; Regolith; Surface; Reflectance; Space weathering
ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; PARTICULATE SURFACES;
SCATTERING; METEORITES; ASTEROIDS; ANALOGS; DAWN; MOON
AB During its year-long orbital mission, the Dawn spacecraft has mapped the surface of main-belt asteroid Vesta multiple times at different spatial resolutions and illumination and viewing angles. The onboard Framing Camera has acquired thousands of clear filter and narrow band images, which, with the availability of high-resolution global shape models, allows for a photometric characterization of the surface in unprecedented detail. We analyze clear filter images to retrieve the photometric properties of the regolith. In the first part of the paper we evaluate different photometric models for the global average. In the second part we use these results to study variations in albedo and steepness of the phase curve over the surface. Maps of these two photometric parameters show large scale albedo variations, which appear to be associated with compositional differences. They also reveal the location of photometrically extreme terrains, where the phase curve is unusually shallow or steep. We find that shallow phase curves are associated with steep slopes on crater walls and faults, as calculated from a shape model. On the other hand, the phase curve of ejecta associated with young impact craters is steep. We interpret these variations in phase curve slope in terms of physical roughness of the regolith. The lack of rough ejecta around older craters suggests that initially rough ejecta associated with impact craters on Vesta are smoothed over a relatively short time of several tens of Myr. We propose that this process is the result of impact gardening, and as such represents a previously unrecognized aspect of Vesta space weathering (Pieters et al., 2012). If this type of space weathering is common, we may expect to encounter this photometric phenomenon on other main belt asteroids. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Schroeder, S. E.; Mottola, S.] Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany.
[Keller, H. U.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
RP Schroder, SE (reprint author), Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany.
EM stefanus.schroeder@dlr.de
RI Schroder, Stefan/D-9709-2013
OI Schroder, Stefan/0000-0003-0323-8324
NR 47
TC 28
Z9 28
U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP 1
PY 2013
VL 85
BP 198
EP 213
DI 10.1016/j.pss.2013.06.009
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 217MR
UT WOS:000324364100015
ER
PT J
AU Gicquel, A
Bockelee-Morvan, D
Leyrat, C
Zakharov, V
Crovisier, J
Biver, N
Gulkis, S
AF Gicquel, Adeline
Bockelee-Morvan, Dominique
Leyrat, Cedric
Zakharov, Vladimir
Crovisier, Jacques
Biver, Nicolas
Gulkis, Samuel
TI Model of dust thermal emission of comet 67P/Churyumov-Gerasimenko for
the Rosetta/MIRO instrument
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Comets; Rosetta; 67P/Churyumov-Gerasimenko; Dust;
Millimeter-submillimeter
ID SPITZER OBSERVATIONS; CONTINUUM EMISSION; MISSION TARGET; NUCLEUS;
GRAINS; ENVIRONMENT; SPECTRA; TRAIL
AB The ESA's Rosetta spacecraft will arrive at comet 67P/Churyumov-Gerasimenko in 2014. The study of gas and dust emission is primary objective of several instruments on the Rosetta spacecraft, including the Microwave Instrument for the Rosetta Orbiter (MIRO). We developed a model of dust thermal emission to estimate the detectability of dust in the vicinity of the nucleus with MIRO. Our model computes the power received by the MIRO antenna in limb viewing as a function of the geometry of the observations and the physical properties of the grains. We show that detection in the millimeter and submillimeter channels. can be achieved near perihelion. (C) 2013 Published by Elsevier Ltd.
C1 [Gicquel, Adeline] LERMA, Observ Paris, F-92195 Meudon, France.
[Bockelee-Morvan, Dominique; Leyrat, Cedric; Crovisier, Jacques; Biver, Nicolas] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92195 Meudon, France.
[Zakharov, Vladimir] Gordien Strato, F-91370 Verrieres Le Buisson, France.
[Gulkis, Samuel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gicquel, A (reprint author), NASA GSFC, Astrochem Lab, Code 691,8880 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM adeline.gicquel@nasa.gov
NR 39
TC 1
Z9 1
U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP 1
PY 2013
VL 85
BP 214
EP 219
DI 10.1016/j.pss.2013.06.008
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 217MR
UT WOS:000324364100016
ER
PT J
AU Nna-Mvondo, D
de la Fuente, JL
Ruiz-Bermejo, M
Khare, B
McKay, CP
AF Nna-Mvondo, Delphine
de la Fuente, Jose L.
Ruiz-Bermejo, Marta
Khare, Bishun
McKay, Christopher P.
TI Thermal characterization of Titan's tholins by simultaneous TG-MS, DTA,
DSC analysis
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Tholin; Titan; Thermogravimetry; Mass spectrometry; Chemical structure;
Thermal degradation
ID LABORATORY SIMULATION; PLASMA DISCHARGE; ORGANIC-MATTER; ATMOSPHERE;
AEROSOLS; HAZE; PYROLYSIS; CHEMISTRY; ANALOGS; POLYACRYLONITRILE
AB Three samples of Titan's tholins synthesized in laboratory under simulated Titan's conditions and presenting different degrees of exposure to ambient atmosphere have been used to study in detail their thermal behavior using thermogravimetry coupled with a mass spectrometer (TG-MS), differential thermal analysis (DTA) and differential scanning calorimetry (DSC). The degradation of Titan's tholins under inert atmosphere follows a three-step consecutive decomposition: a drying stage (>150 degrees C) where moisture is desorbed, this stage indicated the high hydrophilicity of the tholins; a second stage, the main pyrolysis stage (150-575 degrees C) where endothermic decomposition begins releasing mainly ammonia, HCN, acetonitrile, and methane over a broad temperature range. Few other hydrocarbon fragments such as ethylene and propane are released but no cyclic molecules, aliphatic or aromatic, are observed. The last stage (>575 degrees C) is the carbonization of the material leading to a non-crystalline graphitic residue. The thermal degradation under oxygen atmosphere shows the same stages as in argon, with a shift of the thermogravimetric peaks toward lower temperatures indicating a lower thermal stability. The last stage in this case is an oxidative combustion of the char residue. This research concludes that even if Titan tholins, subjected to air contamination for few minutes to several years (varying with the storage conditions) transform to produce different C/N and C/O ratios and thermal stabilities, they undergo the same thermal degradation phases and products. This suggests that the studied three tholins have a similar main chemical structure which does not alter by the air exposure. We discuss on the possible nature of this structure. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Nna-Mvondo, Delphine; Ruiz-Bermejo, Marta] Ctr Astrobiol CSIC INTA, Madrid 28850, Spain.
[de la Fuente, Jose L.] Inst Nacl Tecn Aeroespacial Esteban Terradas INTA, Madrid 28850, Spain.
[Khare, Bishun; McKay, Christopher P.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Khare, Bishun] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Nna-Mvondo, D (reprint author), Univ Nantes 2, Lab Planetol & Geodynam, CNRS, UMR 6112, 2 Rue Houssiniere,BP 92208, F-44322 Nantes 3, France.
EM delphine.nnamvondo@univ-nantes.fr
RI Ruiz-Bermejo, Marta/L-1163-2014
OI Ruiz-Bermejo, Marta/0000-0002-8059-1335
FU Spanish Minister of Economy and Competitiveness (MINECO)
[AYA2009-09288]; Instituto Nacional de Tecnica Aeroespacial "Esteban
Terradas" (INTA); Ministerio de Ciencia e Innovacion (Spain)
[AYA2009-13920-C02-01]
FX D.N.-M. acknowledges the Spanish Minister of Economy and Competitiveness
(MINECO) for financial support under the funded project AYA2009-09288.
J.-L.F. and M.R.-B. have used the research facilities of Centro de
Astrobiologia (CAB) and have been supported by the Instituto Nacional de
Tecnica Aeroespacial "Esteban Terradas" (INTA) and the project
AYA2009-13920-C02-01 of the Ministerio de Ciencia e Innovacion (Spain).
NR 45
TC 9
Z9 9
U1 1
U2 24
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP 1
PY 2013
VL 85
BP 279
EP 288
DI 10.1016/j.pss.2013.06.025
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 217MR
UT WOS:000324364100022
ER
PT J
AU Roatsch, T
Kersten, E
Matz, KD
Preusker, F
Scholten, F
Elgner, S
Jaumann, R
Raymond, CA
Russell, CT
AF Roatsch, Th.
Kersten, E.
Matz, K. -D.
Preusker, F.
Scholten, F.
Elgner, S.
Jaumann, R.
Raymond, C. A.
Russell, C. T.
TI High-resolution Vesta Low Altitude Mapping Orbit Atlas derived from Dawn
Framing Camera images
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Dawn; Vesta; Asteroids; Planetary mapping
AB The Dawn Framing Camera (FC) acquired close to 10,000 clear filter images of Vesta with a resolution of about 20 m/pixel during the Low Altitude Mapping Orbit (LAMO) between December 2011 and April 2012. We ortho-rectified these images and produced a global high-resolution uncontrolled mosaic of Vesta. This global mosaic is the baseline for a high-resolution Vesta atlas that consists of 30 tiles mapped at a scale between 1:200,000 and 1:225,180. The nomenclature used in this atlas was proposed by the Dawn team and was approved by the International Astronomical Union (IAU). The whole atlas is available to the public through the Dawn GIS web page [http://dawn_gis.dlr.de/atlas]. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Roatsch, Th.; Kersten, E.; Matz, K. -D.; Preusker, F.; Scholten, F.; Elgner, S.; Jaumann, R.] German Aerosp Ctr DLR, Inst Planetary Res, Berlin, Germany.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Russell, C. T.] Univ Calif Los Angeles, Inst Geophys, Los Angeles, CA USA.
RP Roatsch, T (reprint author), German Aerosp Ctr DLR, Inst Planetary Res, Berlin, Germany.
EM Thomas.Roatsch@dlr.de
NR 11
TC 13
Z9 13
U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP 1
PY 2013
VL 85
BP 293
EP 298
DI 10.1016/j.pss.2013.06.024
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 217MR
UT WOS:000324364100024
ER
PT J
AU Mohapatra, BR
La Duc, MT
AF Mohapatra, Bidyut R.
La Duc, Myron T.
TI Detecting the dormant: a review of recent advances in molecular
techniques for assessing the viability of bacterial endospores
SO APPLIED MICROBIOLOGY AND BIOTECHNOLOGY
LA English
DT Review
DE Bacillus; Clostridium; Paenibacillus; Spore; Viability
ID IN-SITU HYBRIDIZATION; SPACECRAFT ASSEMBLY FACILITY; BACILLUS-PUMILUS
SAFR-032; PROPIDIUM MONOAZIDE; FLOW-CYTOMETRY; CLOSTRIDIUM-DIFFICILE;
WATER SAMPLES; VIABLE SPORES; HIGH-PRESSURE; SP-NOV
AB Due to their contribution to gastrointestinal and pulmonary disease, their ability to produce various deadly exotoxins, and their resistance to extreme temperature, pressure, radiation, and common chemical disinfecting agents, bacterial endospores of the Firmicutes phylum are a major concern for public and environmental health. In addition, the hardy and dormant nature of endospores renders them a particularly significant threat to the integrity of robotic extraterrestrial life-detection investigations. To prevent the contamination of critical surfaces with seemingly ubiquitous bacterial endospores, clean rooms maintained at exceedingly stringent cleanliness levels (i.e., fewer than 100,000 airborne particles per ft(3)) are used for surgical procedures, pharmaceutical processing and packaging, and fabrication and assembly of medical devices and spacecraft components. However, numerous spore-forming bacterial species have been reported to withstand typical clean room bioreduction strategies (e.g., UV lights, maintained humidity, paucity of available nutrients), which highlights the need for rapid and reliable molecular methods for detecting, enumerating, and monitoring the incidence of viable endospores. Robust means of evaluating and tracking spore burden not only provide much needed information pertaining to endospore ecophysiology in different environmental niches but also empower decontamination and bioreduction strategies aimed at sustaining the reliability and integrity of clean room environments. An overview of recent molecular advances in detecting and enumerating viable endospores, as well as the expanding phylogenetic diversity of pathogenic and clean room-associated spore-forming bacteria, ensues.
C1 [Mohapatra, Bidyut R.; La Duc, Myron T.] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA.
[Mohapatra, Bidyut R.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
RP Mohapatra, BR (reprint author), Louisiana State Univ, Dept Biol Sci, 202 Life Sci Bldg, Baton Rouge, LA 70803 USA.
EM bmohapatra@lsu.edu
FU National Aeronautics and Space Administration
FX The authors thank Dr. K. Venkateswaran for valuable collegial
discussion, advice, and encouragement. 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 114
TC 4
Z9 4
U1 5
U2 64
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0175-7598
EI 1432-0614
J9 APPL MICROBIOL BIOT
JI Appl. Microbiol. Biotechnol.
PD SEP
PY 2013
VL 97
IS 18
BP 7963
EP 7975
DI 10.1007/s00253-013-5115-3
PG 13
WC Biotechnology & Applied Microbiology
SC Biotechnology & Applied Microbiology
GA 209FK
UT WOS:000323739800002
PM 23912118
ER
PT J
AU Riris, H
Rodriguez, M
Allan, GR
Hasselbrack, W
Mao, JP
Stephen, M
Abshire, J
AF Riris, Haris
Rodriguez, Michael
Allan, Graham R.
Hasselbrack, William
Mao, Jianping
Stephen, Mark
Abshire, James
TI Pulsed airborne lidar measurements of atmospheric optical depth using
the Oxygen A-band at 765 nm
SO APPLIED OPTICS
LA English
DT Article
ID DIFFERENTIAL-ABSORPTION LIDAR; CO2 COLUMN ABSORPTION; MODULATION;
PRESSURE; SPECTROSCOPY; SENSITIVITY; ALGORITHM; SPECTRA
AB We report on an airborne demonstration of atmospheric oxygen optical depth measurements with an IPDA lidar using a fiber-based laser system and a photon counting detector. Accurate knowledge of atmospheric temperature and pressure is required for NASA's Active Sensing of CO2 Emissions over Nights, Days, and Seasons (ASCENDS) space mission, and climate modeling studies. The lidar uses a doubled erbium-doped fiber amplifier and single photon-counting detector to measure oxygen absorption at 765 nm. Our results show good agreement between the experimentally derived differential optical depth measurements with the theoretical predictions for aircraft altitudes from 3 to 13 km. (C) 2013 Optical Society of America
C1 [Riris, Haris; Stephen, Mark; Abshire, James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rodriguez, Michael; Allan, Graham R.; Hasselbrack, William] Sigma Space Corp, Lanham, MD 20706 USA.
[Mao, Jianping] Univ Maryland, ESSIC, College Pk, MD 20740 USA.
RP Riris, H (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Haris.Riris@nasa.gov
RI Riris, Haris/D-1004-2013
FU NASA Earth Science Technology Office (ESTO) Instrument Incubator Program
(IIP); NASA ASCENDS Program; Goddard IRAD program
FX We would like to acknowledge the support of the NASA Earth Science
Technology Office (ESTO) Instrument Incubator Program (IIP), the NASA
ASCENDS Program, and the Goddard IRAD program for funding this research.
We would also like to express our appreciation to NASA's Dryden Aircraft
Operations Facility, in Palmdale, California and the DC-8 flight and
ground crews for their support during the flights.
NR 43
TC 10
Z9 10
U1 1
U2 15
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
J9 APPL OPTICS
JI Appl. Optics
PD SEP 1
PY 2013
VL 52
IS 25
BP 6369
EP 6382
DI 10.1364/AO.52.006369
PG 14
WC Optics
SC Optics
GA 211CM
UT WOS:000323881700037
PM 24085100
ER
PT J
AU Munchak, SJ
Skofronick-Jackson, G
AF Munchak, S. Joseph
Skofronick-Jackson, Gail
TI Evaluation of precipitation detection over various surfaces from passive
microwave imagers and sounders
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Passive microwave; Precipitation; Detection; Imager; Sounder;
Emissivity; Variational retrieval
ID EMISSIVITY MODEL; SNOW PARTICLES; LAND; FREQUENCIES; SCATTERING;
RAINFALL; ICE; RETRIEVAL; OCEANS; PARAMETERS
AB During the middle part of this decade, a wide variety of passive microwave imagers and sounders will be unified in the Global Precipitation Measurement (GPM) mission to provide a common basis for frequent (3 h) global precipitation monitoring. The ability of these sensors to detect precipitation by discerning it from non-precipitating background depends upon the channels available and characteristics of the surface and atmosphere. This study quantifies the minimum detectable precipitation rate and fraction of precipitation detected for four representative instruments (TMI, GMI, AMSU-A, and AMSU-B) that will be part of the GPM constellation. Observations for these instruments were constructed from equivalent channels on the SSMIS instrument on DMSP satellites F16 and F17 and matched to precipitation data from NOAA's National Mosaic and QPE (NMQ) during 2009 over the continuous United States. A variational optimal estimation retrieval of non-precipitation surface and atmosphere parameters was used to determine the consistency between the observed brightness temperatures and these parameters, with high cost function values shown to be related to precipitation.
The minimum detectable precipitation rate, defined as the lowest rate for which probability of detection exceeds 50%, and the detected fraction of precipitation are reported for each sensor, surface type (ocean, coast, bare land, snow cover) and precipitation type (rain, mix, snow). The best sensors over ocean and bare land were GMI (0.22 mm h(-1) minimum threshold and 90% of precipitation detected) and AMSU (0.26 mm h(-1) minimum threshold and 81% of precipitation detected), respectively. Over coasts (0.74 mm h(-1) threshold and 12% detected) and snow-covered surfaces (0.44 mm h(-1) threshold and 23% detected), AMSU again performed best but with much lower detection skill, whereas TMI had no skill over these surfaces. The sounders (particularly over water) benefited from the use of re-analysis data (vs. climatology) to set the a priori atmospheric state and all instruments benefited from the use of a conditional snow cover emissivity database over land. It is recommended that real-time sources of these data be used in the operational GPM precipitation algorithms. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Munchak, S. Joseph; Skofronick-Jackson, Gail] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA.
[Munchak, S. Joseph] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Munchak, SJ (reprint author), NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Code 612,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM s.j.munchak@nasa.gov
RI Skofronick-Jackson, Gail/D-5354-2012; Measurement, Global/C-4698-2015
FU NASA [NNX12AD03]; Precipitation Measurement Missions
FX The authors would like to thank Dr. Ramesh Kakar (NASA Headquarters) for
supporting this work through NASA Cooperative Agreement NNX12AD03 and
Precipitation Measurement Missions funding. The authors also extend
their appreciation to Xin Lin for providing the NMQ data set and Felipe
Aires for providing the TELSEM data set.
NR 49
TC 16
Z9 16
U1 2
U2 15
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
J9 ATMOS RES
JI Atmos. Res.
PD SEP
PY 2013
VL 131
SI SI
BP 81
EP 94
DI 10.1016/j.atmosres.2012.10.011
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 212PB
UT WOS:000323994200009
ER
PT J
AU Li, H
Liu, W
Cassell, AM
Kreupl, F
Banerjee, K
AF Li, Hong
Liu, Wei
Cassell, Alan M.
Kreupl, Franz
Banerjee, Kaustav
TI Low-Resistivity Long-Length Horizontal Carbon Nanotube Bundles for
Interconnect Applications-Part I: Process Development
SO IEEE TRANSACTIONS ON ELECTRON DEVICES
LA English
DT Article
DE Carbon nanotubes (CNTs); chemical vapor deposition; contact;
horizontally aligned; interconnects; Manhattan structure; resistivity
ID GLOBAL INTERCONNECTS; PERFORMANCE ANALYSIS; GROWTH; NANOMATERIALS;
CONDUCTIVITY; RELIABILITY; CIRCUIT; DESIGN; ARRAYS; DENSE
AB Although horizontally-aligned carbon nanotube (HACNT) interconnects are the most common scenarios that have been modeled and analyzed in theoretical research, fabrication of HACNT test structures has remained an enigma until now. Through addressing several fabrication challenges, this paper reports a novel process that enables fabrication of high-density, long (over hundred microns), and thick (up to micrometer) HACNT interconnects. Furthermore, horizontal CNT-based 2-D Manhattan structure is demonstrated by properly designing the catalyst and flattening process. These structures are crucial for building angled interconnects and on-chip passive devices. In addition, to address the contact issue between metal and thick HACNT bundles, a multistep lithography combined with specifically designed metal deposition technique is performed to ensure full contact configuration. Using such a process, test structures with arrays of various sizes of HACNT bundle interconnects are fabricated. The process developed in this paper provides an important platform for future research and technology development of CNT-based interconnects and passive elements.
C1 [Li, Hong; Liu, Wei; Banerjee, Kaustav] Univ Calif Santa Barbara, Dept Elect & Comp Engn, Santa Barbara, CA 93106 USA.
[Cassell, Alan M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kreupl, Franz] Tech Univ Munich, Dept Hybrid Elect Syst, D-80333 Munich, Germany.
RP Li, H (reprint author), Micron Technol Inc, Emerging Memory Grp, Boise, ID 83707 USA.
EM hongli@micron.com; liuwei@ece.ucsb.edu; alan.m.cassell@nasa.gov;
franz.kreupl@tum.de; kaustav@ece.ucsb.edu
RI Liu, Wei/B-3584-2015;
OI Kreupl, Franz/0000-0001-5794-9143
FU National Science Foundation [CCF-0811880]
FX Manuscript received February 8, 2013; revised May 15, 2013; accepted May
19, 2013. Date of current version August 19, 2013. This work was
supported by the National Science Foundation under Grant CCF-0811880.
The review of this paper was arranged by Editor A. C. Seabaugh.
NR 42
TC 10
Z9 10
U1 0
U2 32
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9383
J9 IEEE T ELECTRON DEV
JI IEEE Trans. Electron Devices
PD SEP
PY 2013
VL 60
IS 9
BP 2862
EP 2869
DI 10.1109/TED.2013.2275259
PG 8
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA 207YI
UT WOS:000323640300024
ER
PT J
AU Li, H
Liu, W
Cassell, AM
Kreupl, F
Banerjee, K
AF Li, Hong
Liu, Wei
Cassell, Alan M.
Kreupl, Franz
Banerjee, Kaustav
TI Low-Resistivity Long-Length Horizontal Carbon Nanotube Bundles for
Interconnect Applications-Part II: Characterization
SO IEEE TRANSACTIONS ON ELECTRON DEVICES
LA English
DT Article
DE Carbon nanotubes; characterization; horizontally aligned; interconnects;
resistivity; self-heating; temperature coefficient of resistance
ID CONDUCTIVITY; PERFORMANCE; DENSITY; CATALYST; GROWTH; NANOMATERIALS;
RELIABILITY; DIAMETER; DESIGN; ICS
AB Due to the enormous challenges of fabricating long horizontally aligned carbon nanotube (HACNT) bundle interconnects, there exists little research on characterization of long HACNT interconnects. In this paper, taking advantage of our unique HACNT fabrication process outlined in the companion paper, the electrical and self-heating characterization of long HACNT bundles are reported. Negative temperature coefficients of resistance for both per unit length resistance and metal-CNT contact resistance are confirmed from measurements. This first report on the electrical and thermal characterization fills the wide gap between CNT interconnect modeling efforts and corresponding experimental efforts by providing many important extracted parameters that are critical in various modeling and analyses.
C1 [Li, Hong; Liu, Wei; Banerjee, Kaustav] Univ Calif Santa Barbara, Dept Elect & Comp Engn, Santa Barbara, CA 93106 USA.
[Cassell, Alan M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kreupl, Franz] Tech Univ Munich, Dept Hybrid Elect Syst, D-80333 Munich, Germany.
RP Li, H (reprint author), Micron Technol Inc, Emerging Memory Grp, Boise, ID 83707 USA.
EM hongli@micron.com; liuwei@ece.ucsb.edu; alan.m.cassell@nasa.gov;
franz.kreupl@tum.de; kaustav@ece.ucsb.edu
RI Liu, Wei/B-3584-2015;
OI Kreupl, Franz/0000-0001-5794-9143
FU National Science Foundation [CCF-0811880]
FX Manuscript received February 8, 2013; revised July 13, 2013; accepted
July 15, 2013. Date of current version August 19, 2013. This work was
supported by the National Science Foundation under Grant CCF-0811880.
The review of this paper was arranged by Editor A. C. Seabaugh.
NR 33
TC 8
Z9 8
U1 0
U2 21
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9383
J9 IEEE T ELECTRON DEV
JI IEEE Trans. Electron Devices
PD SEP
PY 2013
VL 60
IS 9
BP 2870
EP 2876
DI 10.1109/TED.2013.2275258
PG 7
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA 207YI
UT WOS:000323640300025
ER
PT J
AU Abramowski, A
Acero, F
Aharonian, F
Akhperjanian, AG
Anguner, E
Anton, G
Balenderan, S
Balzer, A
Barnacka, A
Becherini, Y
Tjus, JB
Bernlohr, K
Birsin, E
Bissaldi, E
Biteau, J
Boisson, C
Bolmont, J
Bordas, P
Brucker, J
Brun, F
Brun, P
Bulik, T
Carrigan, S
Casanova, S
Cerruti, M
Chadwick, PM
Chalme-Calvet, R
Chaves, RCG
Cheesebrough, A
Chretien, M
Colafrancesco, S
Cologna, G
Conrad, J
Couturier, C
Dalton, M
Daniel, MK
Davids, ID
Degrange, B
Deil, C
deWilt, P
Dickinson, HJ
Djannati-Atai, A
Domainko, W
Drury, LO
Dubus, G
Dutson, K
Dyks, J
Dyrda, M
Edwards, T
Egberts, K
Eger, P
Espigat, P
Farnier, C
Fegan, S
Feinstein, F
Fernandes, MV
Fernandez, D
Fiasson, A
Fontaine, G
Forster, A
Fussling, M
Gajdus, M
Gallant, YA
Garrigoux, T
Gast, H
Giebels, B
Glicenstein, JF
Goring, D
Grondin, MH
Grudzinska, M
Haffner, S
Hague, JD
Hahn, J
Harris, J
Heinzelmann, G
Henri, G
Hermann, G
Hervet, O
Hillert, A
Hinton, JA
Hofmann, W
Hofverberg, P
Holler, M
Horns, D
Jacholkowska, A
Jahn, C
Jamrozy, M
Janiak, M
Jankowsky, F
Jung, I
Kastendieck, MA
Katarzynski, K
Katz, U
Kaufmann, S
Khelifi, B
Kieffer, M
Klepser, S
Klochkov, D
Kluzniak, W
Kneiske, T
Kolitzus, D
Komin, N
Kosack, K
Krakau, S
Krayzel, F
Kruger, PP
Laffon, H
Lamanna, G
Lefaucheur, J
Lemoine-Goumard, M
Lenain, JP
Lennarz, D
Lohse, T
Lopatin, A
Lu, CC
Marandon, V
Marcowith, A
Maurin, G
Maxted, N
Mayer, M
McComb, TJL
Medina, MC
Mehault, J
Menzler, U
Meyer, M
Moderski, R
Mohamed, M
Moulin, E
Murach, T
Naumann, CL
de Naurois, M
Nedbal, D
Niemiec, J
Nolan, SJ
Oakes, L
Ohm, S
Wilhelmi, ED
Opitz, B
Ostrowski, M
Oya, I
Panter, M
Parsons, RD
Arribas, MP
Pekeur, NW
Pelletier, G
Perez, J
Petrucci, PO
Peyaud, B
Pita, S
Poon, H
Puhlhofer, G
Punch, M
Quirrenbach, A
Raab, S
Raue, M
Reimer, A
Reimer, O
Renaud, M
de los Reyes, R
Rieger, F
Rob, L
Rosier-Lees, S
Rowell, G
Rudak, B
Rulten, CB
Sahakian, V
Sanchez, DA
Santangelo, A
Schlickeiser, R
Schussler, F
Schulz, A
Schwanke, U
Schwarzburg, S
Schwemmer, S
Sol, H
Spengler, G
Spiess, F
Stawarz, L
Steenkamp, R
Stegmann, C
Stinzing, F
Stycz, K
Sushch, I
Szostek, A
Tavernet, JP
Terrier, R
Tluczykont, M
Trichard, C
Valerius, K
van Eldik, C
Vasileiadis, G
Venter, C
Viana, A
Vincent, P
Volk, HJ
Volpe, F
Vorster, M
Wagner, SJ
Wagner, P
Ward, M
Weidinger, M
White, R
Wierzcholska, A
Willmann, P
Wornlein, A
Wouters, D
Zacharias, M
Zajczyk, A
Zdziarski, AA
Zech, A
Zechlin, HS
Perkins, JS
Ojha, R
Stevens, J
Edwards, PG
Kadler, M
AF Abramowski, A.
Acero, F.
Aharonian, F.
Akhperjanian, A. G.
Anguener, E.
Anton, G.
Balenderan, S.
Balzer, A.
Barnacka, A.
Becherini, Y.
Tjus, J. Becker
Bernloehr, K.
Birsin, E.
Bissaldi, E.
Biteau, J.
Boisson, C.
Bolmont, J.
Bordas, P.
Brucker, J.
Brun, F.
Brun, P.
Bulik, T.
Carrigan, S.
Casanova, S.
Cerruti, M.
Chadwick, P. M.
Chalme-Calvet, R.
Chaves, R. C. G.
Cheesebrough, A.
Chretien, M.
Colafrancesco, S.
Cologna, G.
Conrad, J.
Couturier, C.
Dalton, M.
Daniel, M. K.
Davids, I. D.
Degrange, B.
Deil, C.
deWilt, P.
Dickinson, H. J.
Djannati-Atai, A.
Domainko, W.
Drury, L. O'C.
Dubus, G.
Dutson, K.
Dyks, J.
Dyrda, M.
Edwards, T.
Egberts, K.
Eger, P.
Espigat, P.
Farnier, C.
Fegan, S.
Feinstein, F.
Fernandes, M. V.
Fernandez, D.
Fiasson, A.
Fontaine, G.
Foerster, A.
Fuessling, M.
Gajdus, M.
Gallant, Y. A.
Garrigoux, T.
Gast, H.
Giebels, B.
Glicenstein, J. F.
Goering, D.
Grondin, M-H.
Grudzinska, M.
Haeffner, S.
Hague, J. D.
Hahn, J.
Harris, J.
Heinzelmann, G.
Henri, G.
Hermann, G.
Hervet, O.
Hillert, A.
Hinton, J. A.
Hofmann, W.
Hofverberg, P.
Holler, M.
Horns, D.
Jacholkowska, A.
Jahn, C.
Jamrozy, M.
Janiak, M.
Jankowsky, F.
Jung, I.
Kastendieck, M. A.
Katarzynski, K.
Katz, U.
Kaufmann, S.
Khelifi, B.
Kieffer, M.
Klepser, S.
Klochkov, D.
Kluzniak, W.
Kneiske, T.
Kolitzus, D.
Komin, Nu.
Kosack, K.
Krakau, S.
Krayzel, F.
Krueger, P. P.
Laffon, H.
Lamanna, G.
Lefaucheur, J.
Lemoine-Goumard, M.
Lenain, J-P.
Lennarz, D.
Lohse, T.
Lopatin, A.
Lu, C-C.
Marandon, V.
Marcowith, A.
Maurin, G.
Maxted, N.
Mayer, M.
McComb, T. J. L.
Medina, M. C.
Mehault, J.
Menzler, U.
Meyer, M.
Moderski, R.
Mohamed, M.
Moulin, E.
Murach, T.
Naumann, C. L.
de Naurois, M.
Nedbal, D.
Niemiec, J.
Nolan, S. J.
Oakes, L.
Ohm, S.
Wilhelmi, E. de Ona
Opitz, B.
Ostrowski, M.
Oya, I.
Panter, M.
Parsons, R. D.
Arribas, M. Paz
Pekeur, N. W.
Pelletier, G.
Perez, J.
Petrucci, P-O.
Peyaud, B.
Pita, S.
Poon, H.
Puehlhofer, G.
Punch, M.
Quirrenbach, A.
Raab, S.
Raue, M.
Reimer, A.
Reimer, O.
Renaud, M.
de los Reyes, R.
Rieger, F.
Rob, L.
Rosier-Lees, S.
Rowell, G.
Rudak, B.
Rulten, C. B.
Sahakian, V.
Sanchez, D. A.
Santangelo, A.
Schlickeiser, R.
Schuessler, F.
Schulz, A.
Schwanke, U.
Schwarzburg, S.
Schwemmer, S.
Sol, H.
Spengler, G.
Spiess, F.
Stawarz, L.
Steenkamp, R.
Stegmann, C.
Stinzing, F.
Stycz, K.
Sushch, I.
Szostek, A.
Tavernet, J-P.
Terrier, R.
Tluczykont, M.
Trichard, C.
Valerius, K.
van Eldik, C.
Vasileiadis, G.
Venter, C.
Viana, A.
Vincent, P.
Voelk, H. J.
Volpe, F.
Vorster, M.
Wagner, S. J.
Wagner, P.
Ward, M.
Weidinger, M.
White, R.
Wierzcholska, A.
Willmann, P.
Woernlein, A.
Wouters, D.
Zacharias, M.
Zajczyk, A.
Zdziarski, A. A.
Zech, A.
Zechlin, H-S.
Perkins, J. S.
Ojha, R.
Stevens, J.
Edwards, P. G.
Kadler, M.
CA HESS Collaboration
TI HESS and Fermi-LAT discovery of gamma-rays from the blazar 1ES 1312-423
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; galaxies: active; BL Lacertae
objects: individual: 1ES 1312-423; galaxies: jets; gamma-rays: galaxies
ID BL-LACERTAE OBJECTS; LARGE-AREA TELESCOPE; ATMOSPHERIC CHERENKOV
TELESCOPES; SPECTRAL ENERGY-DISTRIBUTIONS; MEDIUM-SENSITIVITY SURVEY;
SOURCE CATALOG; BACKGROUND-RADIATION; COMPLETE SAMPLE; TEV BLAZARS;
RADIO
AB A deep observation campaign carried out by the High Energy Stereoscopic System (HESS) on Centaurus A enabled the discovery of gamma-rays from the blazar 1ES 1312-423, 2 degrees away from the radio galaxy. With a differential flux at 1 TeV of phi(1 TeV) = (1.9 +/- 0.6(stat) +/- 0.4(sys)) x 10(-13) cm(-2) s(-1) TeV-1 corresponding to 0.5 per cent of the Crab nebula differential flux and a spectral index Gamma = 2.9 +/- 0.5(stat) +/- 0.2(sys), 1ES 1312-423 is one of the faintest sources ever detected in the very high energy (E > 100 GeV) extragalactic sky. A careful analysis using three and a half years of Fermi Large Area Telescope (Fermi-LAT) data allows the discovery at high energies (E > 100 MeV) of a hard spectrum (Gamma = 1.4 +/- 0.4(stat) +/- 0.2(sys)) source coincident with 1ES 1312-423. Radio, optical, UV and X-ray observations complete the spectral energy distribution of this blazar, now covering 16 decades in energy. The emission is successfully fitted with a synchrotron self-Compton model for the non-thermal component, combined with a blackbody spectrum for the optical emission from the host galaxy.
C1 [Abramowski, A.; Fernandes, M. V.; Heinzelmann, G.; Horns, D.; Kastendieck, M. A.; Kneiske, T.; Meyer, M.; Opitz, B.; Raue, M.; Spiess, F.; Tluczykont, M.; Zechlin, H-S.] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany.
[Acero, F.; Feinstein, F.; Fernandez, D.; Gallant, Y. A.; Marcowith, A.; Renaud, M.; Vasileiadis, G.; Zajczyk, A.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3,CC 72, F-34095 Montpellier 5, France.
[Aharonian, F.; Bernloehr, K.; Brun, F.; Carrigan, S.; Casanova, S.; Chaves, R. C. G.; Deil, C.; Domainko, W.; Edwards, T.; Eger, P.; Foerster, A.; Gast, H.; Grondin, M-H.; Hague, J. D.; Hahn, J.; Hermann, G.; Hillert, A.; Hofmann, W.; Hofverberg, P.; Krueger, P. P.; Lennarz, D.; Lu, C-C.; Marandon, V.; Wilhelmi, E. de Ona; Panter, M.; Parsons, R. D.; Poon, H.; de los Reyes, R.; Rieger, F.; Sanchez, D. A.; Viana, A.; Voelk, H. J.; Volpe, F.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Aharonian, F.; Drury, L. O'C.] Dublin Inst Adv Studies, Dublin 2, Ireland.
[Aharonian, F.; Akhperjanian, A. G.; Sahakian, V.] Natl Acad Sci Republ Armenia, Yerevan 375019, Armenia.
[Akhperjanian, A. G.; Sahakian, V.] Yerevan Phys Inst, Yerevan 375036, Armenia.
[Anguener, E.; Bernloehr, K.; Birsin, E.; Gajdus, M.; Lohse, T.; Murach, T.; Oakes, L.; Oya, I.; Arribas, M. Paz; Schwanke, U.; Spengler, G.; Sushch, I.; Wagner, P.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Anton, G.; Brucker, J.; Goering, D.; Haeffner, S.; Jahn, C.; Jung, I.; Katz, U.; Lopatin, A.; Raab, S.; Stinzing, F.; Valerius, K.; van Eldik, C.; Willmann, P.; Woernlein, A.] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany.
[Balenderan, S.; Chadwick, P. M.; Cheesebrough, A.; Daniel, M. K.; Harris, J.; McComb, T. J. L.; Nolan, S. J.; Ward, M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Balzer, A.; Klepser, S.; Schulz, A.; Stegmann, C.; Stycz, K.] DESY, D-15735 Zeuthen, Germany.
[Balzer, A.; Fuessling, M.; Holler, M.; Mayer, M.; Stegmann, C.] Univ Potsdam, Inst Phys & Astron, D-14476 Golm, Germany.
[Barnacka, A.; Dyks, J.; Janiak, M.; Kluzniak, W.; Moderski, R.; Rudak, B.; Zajczyk, A.; Zdziarski, A. A.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Becherini, Y.; Cologna, G.; Grondin, M-H.; Jankowsky, F.; Kaufmann, S.; Mohamed, M.; Quirrenbach, A.; Schwemmer, S.; Wagner, S. J.] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany.
[Becherini, Y.; Djannati-Atai, A.; Espigat, P.; Lefaucheur, J.; Pita, S.; Punch, M.; Terrier, R.] Univ Paris Diderot, APC, CNRS, IN2P3,CEA,Irfu,Observat Paris,Sorbonne Paris Cite, F-75205 Paris 13, France.
[Becherini, Y.; Biteau, J.; Degrange, B.; Fegan, S.; Fontaine, G.; Giebels, B.; Khelifi, B.; Laffon, H.; de Naurois, M.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Tjus, J. Becker; Krakau, S.; Menzler, U.; Schlickeiser, R.; Weidinger, M.; Zacharias, M.] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany.
[Bissaldi, E.; Egberts, K.; Kolitzus, D.; Perez, J.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Boisson, C.; Cerruti, M.; Hervet, O.; Rulten, C. B.; Sol, H.; Zech, A.] Univ Paris Diderot, CNRS, Observ Paris, LUTH, F-92190 Meudon, France.
[Bolmont, J.; Chalme-Calvet, R.; Chretien, M.; Couturier, C.; Garrigoux, T.; Jacholkowska, A.; Kieffer, M.; Lenain, J-P.; Naumann, C. L.; Tavernet, J-P.; Vincent, P.] Univ Paris 07, Univ Paris 06, LPNHE, CNRS,IN2P3, F-75252 Paris 5, France.
[Bordas, P.; Klochkov, D.; Puehlhofer, G.; Santangelo, A.; Schwarzburg, S.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Brun, P.; Chaves, R. C. G.; Glicenstein, J. F.; Kosack, K.; Medina, M. C.; Moulin, E.; Peyaud, B.; Schuessler, F.; Wouters, D.] CEA Saclay, DSM, Irfu, F-91191 Gif Sur Yvette, France.
[Bulik, T.; Grudzinska, M.] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland.
[Casanova, S.; Krueger, P. P.; Pekeur, N. W.; Sushch, I.; Venter, C.; Vorster, M.] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa.
[Cerruti, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Colafrancesco, S.] Univ Witwatersrand, Sch Phys, ZA-2050 Johannesburg, South Africa.
[Conrad, J.; Dickinson, H. J.; Farnier, C.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Dalton, M.; Laffon, H.; Lemoine-Goumard, M.; Mehault, J.] Univ Bordeaux 1, Ctr Etud Nuc Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France.
[Davids, I. D.; Steenkamp, R.] Univ Namibia, Dept Phys, Windhoek, Namibia.
[deWilt, P.; Maxted, N.; Rowell, G.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Dubus, G.; Henri, G.; Pelletier, G.; Petrucci, P-O.] UJF Grenoble 1, CNRS, IPAG, INSU, F-38041 Grenoble, France.
[Dutson, K.; Hinton, J. A.; Ohm, S.; White, R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Dyrda, M.; Niemiec, J.] Inst Fizyki Jadrowej PAN, PL-31342 Krakow, Poland.
[Fiasson, A.; Komin, Nu.; Krayzel, F.; Lamanna, G.; Maurin, G.; Rosier-Lees, S.; Trichard, C.] Univ Savoie, Lab Annecy Le Vieux Phys Particules, CNRS, IN2P3, F-74941 Annecy Le Vieux, France.
[Jamrozy, M.; Ostrowski, M.; Szostek, A.; Wierzcholska, A.] Uniwersytet Jagiellonski, Obserwatorium Astronomiczne, PL-30244 Krakow, Poland.
[Katarzynski, K.; Stawarz, L.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland.
[Ohm, S.] Charles Univ Prague, Inst Particle & Nucl Phys, Fac Math & Phys, CZ-18000 Prague 8, Czech Republic.
[Ohm, S.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Perkins, J. S.; Kadler, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Perkins, J. S.; Kadler, M.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Ojha, R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Ojha, R.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
[Stevens, J.] CSIRO Astron & Space Sci, Narrabri, NSW 2390, Australia.
[Edwards, P. G.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
RP Abramowski, A (reprint author), Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany.
EM yvonne.becherini@lsw.uni-heidelberg.de; biteau@in2p3.fr;
david.sanchez@mpi-hd.mpg.de; jeremy.s.perkins@nasa.gov
RI Meyer, Manuel/E-2697-2016; Bissaldi, Elisabetta/K-7911-2016; Drury,
Luke/B-1916-2017; Moulin, Emmanuel/B-5959-2017; Daniel,
Michael/A-2903-2010; Komin, Nukri/J-6781-2015; Casanova,
Sabrina/J-8935-2013; Couturier, Camille/K-7585-2013; Tjus,
Julia/G-8145-2012; Anton, Gisela/C-4840-2013; Katz, Uli/E-1925-2013;
Fontaine, Gerard/D-6420-2014; van Eldik, Christopher/C-3901-2013;
Venter, Christo/E-6884-2011; Reimer, Olaf/A-3117-2013; Schussler,
Fabian/G-5313-2013; Katarzynski, Krzysztof/G-4528-2014; Jamrozy,
Marek/F-4507-2015
OI Meyer, Manuel/0000-0002-0738-7581; Bissaldi,
Elisabetta/0000-0001-9935-8106; Drury, Luke/0000-0002-9257-2270; Moulin,
Emmanuel/0000-0003-4007-0145; de los Reyes Lopez,
Raquel/0000-0003-0485-9552; Daniel, Michael/0000-0002-8053-7910;
Chadwick, Paula/0000-0002-1468-2685; Kneiske, Tanja
M./0000-0002-3210-6200; mohamed, mahmoud/0000-0002-4625-6242; Kruger,
Paulus/0000-0003-0664-8521; Komin, Nukri/0000-0003-3280-0582; Casanova,
Sabrina/0000-0002-6144-9122; Couturier, Camille/0000-0002-0168-1106;
Anton, Gisela/0000-0003-2039-4724; Katz, Uli/0000-0002-7063-4418; van
Eldik, Christopher/0000-0001-9669-645X; Venter,
Christo/0000-0002-2666-4812; Reimer, Olaf/0000-0001-6953-1385;
Schussler, Fabian/0000-0003-1500-6571;
FU German Ministry for Education and Research (BMBF); Max Planck Society;
French Ministry for Research; CNRS-IN2P3; Astroparticle
Interdisciplinary Programme of the CNRS; UK Particle Physics and
Astronomy Research Council (PPARC); IPNP of the Charles University;
South African Department of Science and Technology; National Research
Foundation; University of Namibia; Istituto Nazionale di Astrofisica in
Italy; Centre National d'Etudes Spatiales in France; Commonwealth of
Australia; NASA [NNH09ZDA001N]; NASA post-doctoral Programme at the
Goddard Space Flight Center
FX The support of the Namibian authorities and of the University of Namibia
in facilitating the construction and operation of HESS is gratefully
acknowledged, as is the support by the German Ministry for Education and
Research (BMBF), the Max Planck Society, the French Ministry for
Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary
Programme of the CNRS, the UK Particle Physics and Astronomy Research
Council (PPARC), the IPNP of the Charles University, the South African
Department of Science and Technology and National Research Foundation,
and by the University of Namibia. We appreciate the excellent work of
the technical support staff in Berlin, Durham, Hamburg, Heidelberg,
Palaiseau, Paris, Saclay, and in Namibia in the construction and
operation of the equipment.; 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 ATCA 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. This research was
funded in part by NASA through Fermi Guest Investigator grant
NNH09ZDA001N (proposal number 31263). This research was supported by an
appointment to the NASA post-doctoral Programme at the Goddard Space
Flight Center, administered by Oak Ridge Associated Universities through
a contract with NASA.
NR 82
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SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2013
VL 434
IS 3
BP 1889
EP 1901
DI 10.1093/mnras/stt1081
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 207YE
UT WOS:000323639900006
ER
PT J
AU Kunz, MW
Lesur, G
AF Kunz, Matthew W.
Lesur, Geoffroy
TI Magnetic self-organization in Hall-dominated magnetorotational
turbulence
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; instabilities; MHD; protoplanetary discs;
stars: formation
ID DIFFERENTIALLY ROTATING-DISKS; WEAKLY IONIZED DISKS; MRI CHANNEL FLOWS;
T TAURI DISKS; PROTOPLANETARY DISKS; ACCRETION DISKS; NONLINEAR
EVOLUTION; LINEAR-ANALYSIS; AMBIPOLAR DIFFUSION; PROTOSTELLAR DISKS
AB The magnetorotational instability (MRI) is the most promising mechanism by which angular momentum is efficiently transported outwards in astrophysical discs. However, its application to protoplanetary discs remains problematic. These discs are so poorly ionized that they may not support magnetorotational turbulence in regions referred to as 'dead zones'. It has recently been suggested that the Hall effect, a non-ideal magnetohydrodynamic (MHD) effect, could revive these dead zones by enhancing the magnetically active column density by an order of magnitude or more. We investigate this idea by performing local, three-dimensional, resistive Hall-MHD simulations of the MRI in situations where the Hall effect dominates over Ohmic dissipation. As expected from linear stability analysis, we find an exponentially growing instability in regimes otherwise linearly stable in resistive MHD. However, instead of vigorous and sustained magnetorotational turbulence, we find that the MRI saturates by producing large-scale, long-lived, axisymmetric structures in the magnetic and velocity fields. We refer to these structures as zonal fields and zonal flows, respectively. Their emergence causes a steep reduction in turbulent transport by at least two orders of magnitude from extrapolations based upon resistive MHD, a result that calls into question contemporary models of layered accretion. We construct a rigorous mean-field theory to explain this new behaviour and to predict when it should occur. Implications for protoplanetary disc structure and evolution, as well as for theories of planet formation, are briefly discussed.
C1 [Kunz, Matthew W.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Lesur, Geoffroy] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France.
RP Kunz, MW (reprint author), NASA, Washington, DC 20546 USA.
EM geoffroy.lesur@obs.ujf-grenoble.fr
OI Lesur, Geoffroy/0000-0002-8896-9435
FU NASA [PF1-120084, NAS8-03060]; European Community
[PCIG09-GA-2011-294110]; Rhone-Alpes region [GRANT CPER07_13 CIRA]; NSF
[OCI-1053575]; [TG-AST090105]
FX Support for MWK was provided by NASA through Einstein Post-doctoral
Fellowship Award Number PF1-120084, issued by the Chandra
X-rayObservatory Center, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of NASA under contract
NAS8-03060. GL acknowledges support by the European Community via
contract PCIG09-GA-2011-294110. This work was granted access to the HPC
resources of IDRIS under allocation x2013042231 made by Grand Equipement
National de Calcul Intensif (GENCI). Some of the computations presented
in this paper were performed using the CIMENT infrastructure
(https://ciment.ujf-grenoble.fr), which is supported by the Rhone-Alpes
region (GRANT CPER07_13 CIRA: http://www.ci-ra.org). The Texas Advanced
Computer Center at the University of Texas at Austin also provided HPC
resources under grant number TG-AST090105. This work used the Extreme
Science and Engineering Discovery Environment (XSEDE), which is
supported by NSF grant OCI-1053575. The authors would like to thank Nuno
Loureiro, Jake Simon and Jim Stone for useful conversations, as well as
the expert referee for a prompt and constructive report.
NR 64
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PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2013
VL 434
IS 3
BP 2295
EP 2312
DI 10.1093/mnras/stt1171
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 207YE
UT WOS:000323639900036
ER
PT J
AU Feltre, A
Hatziminaoglou, E
Hernan-Caballero, A
Fritz, J
Franceschini, A
Bock, J
Cooray, A
Farrah, D
Solares, EAG
Ibar, E
Isaak, KG
Lo Faro, B
Marchetti, L
Oliver, SJ
Page, MJ
Rigopoulou, D
Roseboom, IG
Symeonidis, M
Vaccari, M
AF Feltre, A.
Hatziminaoglou, E.
Hernan-Caballero, A.
Fritz, J.
Franceschini, A.
Bock, J.
Cooray, A.
Farrah, D.
Solares, E. A. Gonzalez
Ibar, E.
Isaak, K. G.
Lo Faro, B.
Marchetti, L.
Oliver, S. J.
Page, M. J.
Rigopoulou, D.
Roseboom, I. G.
Symeonidis, M.
Vaccari, M.
TI The roles of star formation and AGN activity of IRS sources in the
HerMES fields
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: starburst; galaxies: star formation;
infrared: galaxies
ID ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE; SPECTRAL
ENERGY-DISTRIBUTIONS; DIGITAL-SKY-SURVEY; SUPERMASSIVE BLACK-HOLES;
PALOMAR-GREEN QUASARS; SIMILAR-TO 2; GALACTIC NUCLEI; MIDINFRARED
SPECTROSCOPY; STARBURST GALAXIES
AB In this work, we explore the impact of the presence of an active galactic nucleus (AGN) on the mid- and far-infrared (IR) properties of galaxies as well as the effects of simultaneous AGN and starburst activity in the same galaxies. To do this, we apply a multicomponent, multiband spectral synthesis technique to a sample of 250 mu m selected galaxies of the Herschel Multi-tiered Extragalactic Survey (HerMES), with Infrared Spectrograph (IRS) spectra available for all galaxies. Our results confirm that the inclusion of the IRS spectra plays a crucial role in the spectral analysis of galaxies with an AGN component improving the selection of the best-fitting hot dust (torus) model.
We find a correlation between the obscured star formation rate, SFRIR, derived from the IR luminosity of the starburst component, and SFRPAH, derived from the luminosity of the PAH features, L-PAH, with SFRFIR taking higher values than SFRPAH. The correlation is different for AGN- and starburst-dominated objects. The ratio of L-PAH to that of the starburst component, L-PAH/L-SB, is almost constant for AGN-dominated objects but decreases with increasing L-SB for starburst-dominated objects. SFRFIR increases with the accretion luminosity, L-acc, with the increase less prominent for the very brightest, unobscured AGN-dominated sources.
We find no correlation between the masses of the hot (AGN-heated) and cold (starburst-heated) dust components. We interpret this as a non-constant fraction of gas driven by the gravitational effects to the AGN while the starburst is ongoing. We also find no evidence of the AGN affecting the temperature of the cold dust component, though this conclusion is mostly based on objects with a non-dominant AGN component. We conclude that our findings do not provide evidence that the presence of AGN affects the star formation process in the host galaxy, but rather that the two phenomena occur simultaneously over a wide range of luminosities.
C1 [Feltre, A.; Franceschini, A.; Marchetti, L.] Univ Padua, Dipartimento Fis Astron, I-35122 Padua, Italy.
[Feltre, A.; Hatziminaoglou, E.] ESO, D-85748 Garching, Germany.
[Hernan-Caballero, A.] CSIC UC, Inst Fis Cantabria, E-39005 Santander, Spain.
[Fritz, J.] Univ Ghent, Vakgrp Fys Sterrenkunde, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Bock, J.; Cooray, A.] CALTECH, Pasadena, CA 91125 USA.
[Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Solares, E. A. Gonzalez] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ibar, E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Isaak, K. G.] ESTEC SRE SA, ESA Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands.
[Marchetti, L.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Roseboom, I. G.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Rigopoulou, D.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England.
[Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Roseboom, I. G.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh, Midlothian, Scotland.
[Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, Cape Town, South Africa.
RP Feltre, A (reprint author), Univ Padua, Dipartimento Fis Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy.
EM afeltre@eso.org
RI Vaccari, Mattia/R-3431-2016;
OI Vaccari, Mattia/0000-0002-6748-0577; Marchetti,
Lucia/0000-0003-3948-7621
FU Alfred P. Sloan Foundation; National Aeronautics and Space
Administration; National Science Foundation; US Department of Energy;
Japanese Monbukagakusho; Max Planck Society; NASA; JPL; CSA (Canada);
NAOC (China); CEA, France; CNES, France; CNRS (France); ASI (Italy);
MCINN (Spain); SNSB (Sweden); STFC, UK; UKSA (UK); NASA (USA)
FX Funding for the creation and distribution of the SDSS Archive 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 website is
http://www.sdss.org/.; SPIRE has been developed by a consortium of
institutes led by Cardiff Univ. (UK), 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).;
The Cornell Atlas of Spitzer/IRS Sources (CASSIS) is a product of the
Infrared Science Center at Cornell University, supported by NASA and
JPL.
NR 84
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2013
VL 434
IS 3
BP 2426
EP 2437
DI 10.1093/mnras/stt1177
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 207YE
UT WOS:000323639900046
ER
PT J
AU Ramsay, G
Doyle, JG
Hakala, P
Garcia-Alvarez, D
Brooks, A
Barclay, T
Still, M
AF Ramsay, Gavin
Doyle, J. Gerry
Hakala, Pasi
Garcia-Alvarez, David
Brooks, Adam
Barclay, Thomas
Still, Martin
TI Short-duration high-amplitude flares detected on the M dwarf star KIC
5474065
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE astrobiology; magnetic reconnection; stars: activity; stars: flare;
stars: individual: KIC 5474065; stars: individual: KIC 9726699
ID WHITE-LIGHT FLARES; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; UV CETI;
STELLAR FLARES; STATISTICAL-ANALYSIS; OPTICAL PHOTOMETRY; OBSERVATIONAL
DATA; MAGNETIC ACTIVITY; OPEA MODEL
AB Using data obtained during the RATS-Kepler project, we identified one short-duration flare in a 1 h sequence of ground-based photometry of the dwarf star KIC 5474065. Observations made using Gran Telescopio Canarias show that it is a star with an M4V spectral type. Kepler observations made using 1 min sampling show that KIC 5474065 exhibits large-amplitude (delta F/F > 0.4) optical flares which have a duration as short as 10 min. We compare the energy distribution of flares from KIC 5474065 with that of KIC 9726699, which has also been observed using 1-min sampling, and ground-based observations of other M dwarf stars in the literature. We discuss the possible implications these short-duration, relatively low-energy flares would have on the atmosphere of exoplanets orbiting in the habitable zone of these flare stars.
C1 [Ramsay, Gavin; Doyle, J. Gerry; Brooks, Adam] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Hakala, Pasi] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland.
[Garcia-Alvarez, David] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Garcia-Alvarez, David] Univ La Laguna, Dpto Astrofs, E-38205 Tenerife, Spain.
[Garcia-Alvarez, David] Grantecan CALP, E-38712 Brena Baja, La Palma, Spain.
[Brooks, Adam] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
RP Ramsay, G (reprint author), Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland.
EM gar@arm.ac.uk
FU NASA Science Mission Directorate; NASA [NAS5-26555]; NASA Office of
Space Science [NNX09AF08G]; Northern Ireland Government through
Department of Culture, Arts and Leisure
FX This paper includes data collected by the Kepler mission. Funding for
the Kepler mission is provided by the NASA Science Mission Directorate.
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. Observations were also made with the GTC,
installed in the Spanish Observatorio del Roque de los Muchachos of the
Instituto de Astrofisica de Canarias, in the island of La Palma. Armagh
Observatory is supported by the Northern Ireland Government through the
Department of Culture, Arts and Leisure. We thank the referee for a
constructive and helpful report.
NR 59
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2013
VL 434
IS 3
BP 2451
EP 2457
DI 10.1093/mnras/stt1182
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 207YE
UT WOS:000323639900048
ER
PT J
AU Tombesi, F
Reeves, JN
Reynolds, CS
Garcia, J
Lohfink, A
AF Tombesi, F.
Reeves, J. N.
Reynolds, C. S.
Garcia, J.
Lohfink, A.
TI An outburst scenario for the X-ray spectral variability in 3C 111
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; line: identification;
plasmas; galaxies: active; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; ACCRETION DISC OUTFLOWS; LINE RADIO GALAXIES;
ULTRA-FAST OUTFLOWS; ADVECTION-DOMINATED ACCRETION; SHELL
ABSORPTION-LINES; XMM-NEWTON OBSERVATION; SPINNING BLACK-HOLE;
SEYFERT-GALAXIES; SUZAKU VIEW
AB We present a combined Suzaku and Swift BAT broad-band E = 0.6-200 keV spectral analysis of three 3C 111 observations obtained in 2010. The data are well described with an absorbed power-law continuum and a weak (R similar or equal to 0.2) cold reflection component from distant material. We constrain the continuum cutoff at E-C similar or equal to 150-200 keV, which is in accordance with X-ray Comptonization corona models and supports claims that the jet emission is only dominant at much higher energies. Fe xxvi Ly alpha emission and absorption lines are also present in the first and second observations, respectively. The modelling and interpretation of the emission line is complex and we explore three possibilities. If originating from ionized-disc reflection, this should be emitted at r(in) >= 50 r(g) or, in the lamp-post configuration, the illuminating source should be at a height of h >= 30 r(g) above the black hole. Alternatively, the line could be modelled with a hot collisionally ionized plasma with temperature kT = 22.0(-3.2)(+6.1) keV or a photoionized plasma with log xi = 4.52(-0.16)(+0.10)erg s(-1) cm and column density N-H > 3 x 10(23) cm(-2). However, the first and second scenarios are less favoured on statistical and physical grounds, respectively. The blueshifted absorption line in the second observation can be modelled as an ultrafast outflow (UFO) with ionization parameter log xi = 4.47(-0.04)(+0.76)erg s(-1) cm, column density N-H = (5.3(-1.3)(+1.8)) x 10(22) cm(-2) and outflow velocity v(out) = 0.104 +/- 0.006c. Interestingly, the parameters of the photoionized emission model remarkably match those of the absorbing UFO, supporting the possibility that the same material could be responsible for both emission and absorption. We suggest an outburst scenario in which an accretion disc wind, initially lying out of the line of sight and observed in emission, then crosses our view to the source and it is observed in absorption as a mildly relativistic UFO.
C1 [Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Tombesi, F.; Reynolds, C. S.; Garcia, J.; Lohfink, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Reeves, J. N.] Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England.
[Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Tombesi, F (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
EM ftombesi@astro.umd.edu
RI XRAY, SUZAKU/A-1808-2009
FU National Aeronautics and Space Administration [NNX12AH40G]; Astrophysics
Data Analysis Program, part of the ROSES
FX The authors thank the referee for the thorough reading and the
constructive comments that led to improvements in the paper. FT thank K.
Fukumura, D. Kazanas, R. Nemmen, R. F. Mushotzky, S. B. Kraemer, M.
Cappi and H. L. Marshall for the useful discussions. FT acknowledges
partial support for this work by the National Aeronautics and Space
Administration under Grant No. NNX12AH40G issued through the
Astrophysics Data Analysis Program, part of the ROSES 2010.
NR 127
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2013
VL 434
IS 3
BP 2707
EP 2717
DI 10.1093/mnras/stt1213
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 207YE
UT WOS:000323639900071
ER
PT J
AU Schutte, CA
Hunter, K
Mckay, P
Di Iorio, D
Joye, SB
Meile, C
AF Schutte, Charles A.
Hunter, Kimberley
Mckay, Paul
Di Iorio, Daniela
Joye, Samantha B.
Meile, Christof
TI Patterns and Controls of Nutrient Concentrations in a Southeastern
United States Tidal Creek
SO OCEANOGRAPHY
LA English
DT Article
ID DISSOLVED ORGANIC-CARBON; SALT-MARSH ESTUARY; NITROGEN; EXPORT;
PHOSPHORUS; LIMITATION; DISCHARGE; SEDIMENT; ZONES
AB Terrestrial inputs largely govern nutrient delivery to the coastal ocean, and subsequent processes transform these nutrients in the land-ocean transition zone. Here, we describe spatial and temporal patterns in surface water chemistry from the Duplin, a salt marsh/tidal creek system located in coastal Georgia, USA. Key drivers of nutrient concentration patterns in the Duplin include discharge from the nearby Altamaha River, groundwater inputs, exchange with the marsh platform, and biological processes within the tidal creek. Altamaha River discharge is correlated with salinity in the Duplin, but the processes taking place within the Duplin watershed regulate the distribution of other dissolved and particulate materials. Long-term data sets advance our understanding of the relative importance of these processes in generating the observed patterns in surface water chemistry. This knowledge improves our ability to predict how coastal systems will respond to anthropogenic perturbations.
C1 [Schutte, Charles A.; Hunter, Kimberley; Di Iorio, Daniela; Joye, Samantha B.; Meile, Christof] Univ Georgia, Athens, GA 30602 USA.
[Mckay, Paul] Stennis Space Ctr, Naval Res Lab, Stennis Space Ctr, MS USA.
RP Schutte, CA (reprint author), Univ Georgia, Athens, GA 30602 USA.
EM mjoye@uga.edu; cmeile@uga.edu
OI Schutte, Charles/0000-0002-3907-7828; Meile,
Christof/0000-0002-0825-4596; Joye, Samantha/0000-0003-1610-451X
FU NSF [OCE 99-82133, OCE 06-20959, OCE 12-37140]
FX We thank the GCE LTER technicians (D. Saucedo, J. Shalack, C. Reddy, A.
Nix) for Duplin sample collection, W. Porubsky and N. Weston for
groundwater sampling, and W Sheldon for database maintenance. This study
was supported by the NSF funded Georgia Coastal Ecosystems Long Term
Ecological Research program (OCE 99-82133, OCE 06-20959, and OCE
12-37140) to S.B.J., C.M. and D.D.
NR 35
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U1 4
U2 30
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD SEP
PY 2013
VL 26
IS 3
SI SI
BP 132
EP 139
PG 8
WC Oceanography
SC Oceanography
GA 210DD
UT WOS:000323808600019
ER
PT J
AU Saleeb, AF
Dhakal, B
Padula, SA
Gaydosh, DJ
AF Saleeb, A. F.
Dhakal, B.
Padula, S. A., II
Gaydosh, D. J.
TI Calibration of SMA material model for the prediction of the
'evolutionary' load-bias behavior under conditions of extended thermal
cycling
SO SMART MATERIALS AND STRUCTURES
LA English
DT Article; Proceedings Paper
CT ASME Conference on Smart Materials, Adaptive Structures and Intelligent
Systems
CY SEP 19-21, 2012
CL Stone Mountain, GA
SP ASME, Gen Motors, Parker Hannifin, Dynalloy Inc, Teledyne Sci & Imag, IOP Publishing, Sage Publish, NextGen Aeronaut, Natl Sci Fdn, Air Force Off Sci Res
ID SHAPE-MEMORY ALLOYS; THERMOMECHANICAL BEHAVIOR; CONSTITUTIVE MODEL; NITI
ALLOYS; SIMULATIONS
AB This work is focused on the characterization of the cyclic response of the 55NiTi polycrystalline material system using a recently formulated, multimechanism-based, modeling framework. It has a number of significant contributions. First, it presents a comprehensive characterization of such a complex material system under broad thermo-mechanical loading conditions in isobaric experiments that cover: (a) the entire relevant stress range from 10 to 300 MPa, and (b) sufficient number of thermal cycles to enable the investigation of the details of the evolution of the cyclic strain-versus-temperature hysteresis loops. Second, the detailed comparisons presented for the model results and the experimental measurements provide the necessary validation of the modeling capabilities of the multimechanism framework. Third, specific plots are given detailing the variations with thermal cycling of the internal variables associated with each of the individual inelastic mechanisms. Fourth, an anatomical discussion details the interplay between the internal mechanisms to describe the material behavior within all the important response characteristic regions, thus providing a convenient means to complement the theoretical concepts in the mathematical approach. Given the comprehensive nature of this model, and its successful experimental validation under a wide range of conditions, it is believed that the model is capable of analyzing 55NiTi actuators. It is also emphasized that the insights provided in this work will carry forth to characterization of other SMA material systems.
C1 [Saleeb, A. F.; Dhakal, B.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
[Padula, S. A., II] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Gaydosh, D. J.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
RP Saleeb, AF (reprint author), Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
EM saleeb@uakron.edu; bd27@zips.uakron.edu; santo.a.padula@nasa.gov;
darrell.j.gaydosh@nasa.gov
FU NASA, Fundamental Aeronautics Program, Subsonic, Fixed-Wing
[NNH10ZEA001N-SFW1, NNX11AI57A]
FX This work was supported by NASA, Fundamental Aeronautics Program,
Subsonic, Fixed-Wing, Project No. NNH10ZEA001N-SFW1, Grant No:
NNX11AI57A to the University of Akron. The authors would like to
acknowledge Drs S M Arnold and Ronald Noebe for their technical guidance
and programmatic support during the different phases of the project.
NR 20
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U1 1
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0964-1726
EI 1361-665X
J9 SMART MATER STRUCT
JI Smart Mater. Struct.
PD SEP
PY 2013
VL 22
IS 9
AR 094017
DI 10.1088/0964-1726/22/9/094017
PG 13
WC Instruments & Instrumentation; Materials Science, Multidisciplinary
SC Instruments & Instrumentation; Materials Science
GA 210KP
UT WOS:000323832000019
ER
PT J
AU Saleeb, AF
Dhakal, B
Hosseini, MS
Padula, SA
AF Saleeb, A. F.
Dhakal, B.
Hosseini, M. S.
Padula, S. A., II
TI Large scale simulation of NiTi helical spring actuators under repeated
thermomechanical cycles
SO SMART MATERIALS AND STRUCTURES
LA English
DT Article; Proceedings Paper
CT ASME Conference on Smart Materials, Adaptive Structures and Intelligent
Systems
CY SEP 19-21, 2012
CL Stone Mountain, GA
SP ASME, Gen Motors, Parker Hannifin, Dynalloy Inc, Teledyne Sci & Imag, IOP Publishing, Sage Publish, NextGen Aeronaut, Natl Sci Fdn, Air Force Off Sci Res
ID SHAPE-MEMORY ALLOYS; CONSTITUTIVE MODEL; BEHAVIOR; DEFORMATION; STRAIN;
IMPLEMENTATION; COMPRESSION; ASYMMETRY; TENSION; SMAS
AB As typically utilized in applications, a shape memory alloy (SMA) actuator operates under a large number of thermomechanical cycles, hence the importance of accounting for the cyclic behavior characteristics in modeling and numerical simulation of these actuators. To this end, the present work is focused on the characterization of the cyclic, evolutionary behavior of binary 55NiTi using a newly developed, multi-axial, material-modeling framework and its finite element analysis (FEA) implementation for use in the simulations of SMA actuators. In particular, two different geometric configurations of four-and two-coil helical springs subjected to axial end-forces are investigated under the effect of a large number of thermal cycles leading to the saturated deformation state of the coils. In addition, two different boundary conditions were examined, corresponding to: (a) the loading end cross section assumed to be free-to-twist, and (b) the loading end cross section assumed to be restrained against twist rotation. The study has led to the following five important conclusions: (i) the states of stresses and strains in the coils exhibited marked spatial non-homogeneities, both along the length as well as the cross section of the wires; (ii) the cyclic deformation response of the coils exhibits a similar evolutionary character to that of the 55NiTi material when tested under simple isobaric tensile stress conditions; (iii) the end boundary conditions affect the evolution of the deformation response; (iv) the magnitudes of the evolving nonlinear deformation states (i.e., axial displacements on the martensite and austenite sides, as well as the actuation displacement) were found to be proportional to the number of coils in an essentially linear manner, and (v) the change in coil diameter, while maintaining the pitch height, wire diameter and the number of coils fixed, has a significant effect on the response of the helical spring, both with regard to the resulting stress state and the evolutionary axial displacement behavior during the thermal cycles.
C1 [Saleeb, A. F.; Dhakal, B.; Hosseini, M. S.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
[Padula, S. A., II] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Saleeb, AF (reprint author), Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
EM saleeb@uakron.edu
FU Fundamental Aeronautics Program, Subsonic, Fixed-Wing [NNH10ZEA001
N-SFW1, NNX11AI57A]
FX This work was supported by the Fundamental Aeronautics Program,
Subsonic, Fixed-Wing, Project No. NNH10ZEA001 N-SFW1, Grant No:
NNX11AI57A to the University of Akron. The authors would like to
acknowledge Drs S M Arnold and Ronald Noebe for their technical guidance
and programmatic support during the different phases of the project.
NR 49
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U1 1
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0964-1726
EI 1361-665X
J9 SMART MATER STRUCT
JI Smart Mater. Struct.
PD SEP
PY 2013
VL 22
IS 9
AR 094006
DI 10.1088/0964-1726/22/9/094006
PG 20
WC Instruments & Instrumentation; Materials Science, Multidisciplinary
SC Instruments & Instrumentation; Materials Science
GA 210KP
UT WOS:000323832000008
ER
PT J
AU Loth, E
Titchener, N
Babinsky, H
Povinelli, L
AF Loth, Eric
Titchener, Neil
Babinsky, Holger
Povinelli, Louis
TI Canonical Normal Shock Wave/Boundary-Layer Interaction Flows Relevant to
External Compression Inlets
SO AIAA JOURNAL
LA English
DT Article
ID VORTEX GENERATORS; SEPARATION; DIFFUSER
AB The normal shock wave/boundary-layer interaction is important to the operation and performance of a supersonic inlet, and the normal shock wave/boundary-layer interaction is particularly prominent in external compression inlets. To improve understanding of such interactions, it is helpful to make use of fundamental flows that capture the main elements of inlets, without resorting to the level of complexity and system integration associated with full-geometry inlets. In this paper, several fundamental flowfleld configurations have been considered as possible test cases to represent the normal shock wave/boundary-layer interaction aspects found in typical external compression inlets, and it was found that the spillage diffuser more closely retains the basic flow features of an external compression inlet than the other configurations. In particular, this flowfield allows the normal shock Mach number as well as the amount and rate of subsonic diffusion to all be held approximately constant and independent of the application of flow control. In addition, a survey of several external compression inlets was conducted to quantify the flow and geometric parameters of the spillage diffuser relevant to actual inlets. The results indicated that such a flow may be especially relevant if the terminal Mach number is about 1.3 to 1.4, the confinement parameter is around 10%, and the width is around twice or three times the height. In addition, the area expansion downstream of the shock should be limited to the conservative side of incipient stall based on incompressible diffusers.
C1 [Loth, Eric] Univ Virginia, Charlottesville, VA 22904 USA.
[Titchener, Neil; Babinsky, Holger] Univ Cambridge, Cambridge CB2 1PZ, England.
[Povinelli, Louis] NASA, John H Glenn Res Ctr Lewis Field, Prop Syst Div, Cleveland, OH 44135 USA.
RP Loth, E (reprint author), Univ Virginia, Charlottesville, VA 22904 USA.
NR 54
TC 2
Z9 3
U1 1
U2 17
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD SEP
PY 2013
VL 51
IS 9
BP 2208
EP 2217
DI 10.2514/1.J052175
PG 10
WC Engineering, Aerospace
SC Engineering
GA 207HL
UT WOS:000323589400013
ER
PT J
AU Derkevorkian, A
Masri, SF
Alvarenga, J
Boussalis, H
Bakalyar, J
Richards, WL
AF Derkevorkian, Armen
Masri, Sami F.
Alvarenga, Jessica
Boussalis, Helen
Bakalyar, John
Richards, W. Lance
TI Strain-Based Deformation Shape-Estimation Algorithm for Control and
Monitoring Applications
SO AIAA JOURNAL
LA English
DT Article
ID FIBER-OPTIC SENSORS; BRAGG-GRATING SENSORS; ADVANCED
COMPOSITE-MATERIALS; PANELS; ARRAY
AB A new deformation shape-sensing methodology is investigated for the purposes of real-time condition assessment, control, and health monitoring of flexible lightweight aerospace structures. The fiber optic strain sensing technology was recently proposed by the NASA Dryden Flight Research Center. The methodology implements the use of fiber optic sensors to obtain strain measurements from the target structure and to estimate the corresponding displacement field. In this paper, the methodology is investigated through an experimental aluminum winglike swept-plate model. The proposed algorithm is implemented for three distinct loading cases and compared to a well-established modal-based shape-estimation algorithm. The estimation results from both methods are also compared to reference displacements from photogrammetry and computational analyses. The estimation error for each method is quantified using the root-mean-square measure, and the range of validity of the approach for damage detection is established. Furthermore, the disadvantages and the advantages of each method are discussed, demonstrating the additional benefits of using the proposed fiber optic strain sensing methodology to achieve a robust method for monitoring ultra-lightweight flying wings or next-generation commercial airplanes.
C1 [Derkevorkian, Armen; Masri, Sami F.] Univ So Calif, Viterbi Sch Engn, Los Angeles, CA 90089 USA.
[Alvarenga, Jessica] Calif State Univ Los Angeles, NASA URC SPACE Ctr, Los Angeles, CA 90032 USA.
[Boussalis, Helen] Calif State Univ Los Angeles, NASA URC SPACE Ctr, Coll Engn, Los Angeles, CA 90032 USA.
[Bakalyar, John; Richards, W. Lance] NASA Dryden Flight Res Ctr, Edwards AFB, CA 93524 USA.
RP Derkevorkian, A (reprint author), Univ So Calif, Viterbi Sch Engn, 3620 South Vermont Ave,KAP268B, Los Angeles, CA 90089 USA.
FU NASA [URC NCC NNX08BA44A]
FX This work was supported by NASA Grant URC NCC NNX08BA44A.
NR 41
TC 21
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U1 1
U2 23
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 SEP
PY 2013
VL 51
IS 9
BP 2231
EP 2240
DI 10.2514/1.J052215
PG 10
WC Engineering, Aerospace
SC Engineering
GA 207HL
UT WOS:000323589400015
ER
PT J
AU Adams, ER
Ciardi, DR
Dupree, AK
Gautier, TN
Kulesa, C
McCarthy, D
AF Adams, E. R.
Ciardi, D. R.
Dupree, A. K.
Gautier, T. N., III
Kulesa, C.
McCarthy, D.
TI ADAPTIVE OPTICS IMAGES OF KEPLER OBJECTS OF INTEREST (vol 144, 42, 2012)
SO ASTRONOMICAL JOURNAL
LA English
DT Correction
C1 [Adams, E. R.; Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ciardi, D. R.] NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Gautier, T. N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kulesa, C.; McCarthy, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Adams, ER (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 1
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2013
VL 146
IS 3
AR 71
DI 10.1088/0004-6256/146/3/71
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 203OO
UT WOS:000323302700028
ER
PT J
AU Jiang, P
Ge, J
Cargile, P
Crepp, JR
De Lee, N
de Mello, GFP
Esposito, M
Ferreira, LD
Femenia, B
Fleming, SW
Gaudi, BS
Ghezzi, L
Hernandez, JIG
Hebb, L
Lee, BL
Ma, B
Stassun, KG
Wang, J
Wisniewski, JP
Agol, E
Bizyaev, D
Brewington, H
Chang, L
da Costa, LN
Eastman, JD
Ebelke, G
Gary, B
Kane, SR
Li, R
Liu, J
Mahadevan, S
Maia, MAG
Malanushenko, V
Malanushenko, E
Muna, D
Nguyen, DC
Ogando, RLC
Oravetz, A
Oravetz, D
Pan, KK
Pepper, J
Paegert, M
Prieto, CA
Rebolo, R
Santiago, BX
Schneider, DP
Bradley, ACS
Sivarani, T
Snedden, S
van Eyken, JC
Wan, XK
Weaver, BA
Zhao, B
AF Jiang, Peng
Ge, Jian
Cargile, Phillip
Crepp, Justin R.
De Lee, Nathan
Porto de Mello, Gustavo F.
Esposito, Massimiliano
Ferreira, Leticia D.
Femenia, Bruno
Fleming, Scott W.
Gaudi, B. Scott
Ghezzi, Luan
Gonzalez Hernandez, Jonay I.
Hebb, Leslie
Lee, Brian L.
Ma, Bo
Stassun, Keivan G.
Wang, Ji
Wisniewski, John P.
Agol, Eric
Bizyaev, Dmitry
Brewington, Howard
Chang, Liang
da Costa, Luiz Nicolaci
Eastman, Jason D.
Ebelke, Garrett
Gary, Bruce
Kane, Stephen R.
Li, Rui
Liu, Jian
Mahadevan, Suvrath
Maia, Marcio A. G.
Malanushenko, Viktor
Malanushenko, Elena
Muna, Demitri
Duy Cuong Nguyen
Ogando, Ricardo L. C.
Oravetz, Audrey
Oravetz, Daniel
Pan, Kaike
Pepper, Joshua
Paegert, Martin
Allende Prieto, Carlos
Rebolo, Rafael
Santiago, Basilio X.
Schneider, Donald P.
Bradley, Alaina C. Shelden
Sivarani, Thirupathi
Snedden, Stephanie
van Eyken, J. C.
Wan, Xiaoke
Weaver, Benjamin A.
Zhao, Bo
TI VERY LOW MASS STELLAR AND SUBSTELLAR COMPANIONS TO SOLAR-LIKE STARS FROM
MARVELS. IV. A CANDIDATE BROWN DWARF OR LOW-MASS STELLAR COMPANION TO
HIP 67526
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: spectroscopic; brown dwarfs; stars: individual (HIP 67526);
stars: low-mass; techniques: radial velocities
ID FIXED-DELAY INTERFEROMETER; EXTERNALLY DISPERSED INTERFEROMETER;
EXTRASOLAR PLANET DETECTION; ALL-SKY SURVEY; SHORT-PERIOD; GIANT
PLANETS; STATISTICAL PROPERTIES; ORBITAL ELEMENTS; ACCURATE MASSES;
ADAPTIVE OPTICS
AB We report the discovery of a candidate brown dwarf (BD) or a very low mass stellar companion (MARVELS-5b) to the star HIP 67526 from the Multi-object Apache point observatory Radial Velocity Exoplanet Large-area Survey (MARVELS). The radial velocity curve for this object contains 31 epochs spread over 2.5 yr. Our Keplerian fit, using a Markov Chain Monte Carlo approach, reveals that the companion has an orbital period of 90.2695(-0.0187)(+0.0188) days, an eccentricity of 0.4375 +/- 0.0040, and a semi-amplitude of 2948.14(-16.55)(+16.65) m s(-1). Using additional high-resolution spectroscopy, we find the host star has an effective temperature T-eff = 6004 +/- 34 K, a surface gravity log g (cgs) = 4.55 +/- 0.17, and a metallicity [Fe/H] = +0.04 +/- 0.06. The stellar mass and radius determined through the empirical relationship of Torres et al. yields 1.10 +/- 0.09 M-circle dot and 0.92 +/- 0.19 R-circle dot. The minimum mass of MARVELS-5b is 65.0 +/- 2.9 M-Jup, indicating that it is likely to be either a BD or a very low mass star, thus occupying a relatively sparsely populated region of the mass function of companions to solar-type stars. The distance to this system is 101 +/- 10 pc from the astrometric measurements of Hipparcos. No stellar tertiary is detected in the high-contrast images taken by either FastCam lucky imaging or Keck adaptive optics imaging, ruling out any star with mass greater than 0.2 M-circle dot at a separation larger than 40 AU.
C1 [Jiang, Peng; Ge, Jian; De Lee, Nathan; Fleming, Scott W.; Lee, Brian L.; Ma, Bo; Wang, Ji; Chang, Liang; Mahadevan, Suvrath; Duy Cuong Nguyen; Sivarani, Thirupathi; Wan, Xiaoke; Zhao, Bo] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Jiang, Peng] Chinese Acad Sci, Univ Sci & Technol China, Key Lab Res Galaxies & Cosmol, Hefei 230026, Anhui, Peoples R China.
[Cargile, Phillip; De Lee, Nathan; Hebb, Leslie; Stassun, Keivan G.; Gary, Bruce; Pepper, Joshua; Paegert, Martin] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Porto de Mello, Gustavo F.; Ferreira, Leticia D.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, RJ, Brazil.
[Esposito, Massimiliano; Femenia, Bruno; Gonzalez Hernandez, Jonay I.; Allende Prieto, Carlos; Rebolo, Rafael] Lab Interinst E Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Esposito, Massimiliano; Femenia, Bruno; Gonzalez Hernandez, Jonay I.; Allende Prieto, Carlos] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Fleming, Scott W.; Mahadevan, Suvrath; Schneider, Donald P.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Fleming, Scott W.; Mahadevan, Suvrath; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Gaudi, B. Scott; Eastman, Jason D.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Ghezzi, Luan; da Costa, Luiz Nicolaci; Maia, Marcio A. G.; Ogando, Ricardo L. C.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Porto de Mello, Gustavo F.; Ferreira, Leticia D.; Ghezzi, Luan; da Costa, Luiz Nicolaci; Maia, Marcio A. G.; Ogando, Ricardo L. C.; Santiago, Basilio X.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Lee, Brian L.; Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
[Wisniewski, John P.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Bizyaev, Dmitry; Brewington, Howard; Ebelke, Garrett; Malanushenko, Viktor; Malanushenko, Elena; Oravetz, Audrey; Oravetz, Daniel; Pan, Kaike; Bradley, Alaina C. Shelden; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA.
[Eastman, Jason D.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Eastman, Jason D.] Univ Calif Santa Barbara, Dept Phys Broida Hall, Santa Barbara, CA 93106 USA.
[Kane, Stephen R.; van Eyken, J. C.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Muna, Demitri; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY USA.
[Rebolo, Rafael] CSIC, E-28006 Madrid, Spain.
[Santiago, Basilio X.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil.
[Sivarani, Thirupathi] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
RP Jiang, P (reprint author), Univ Florida, Dept Astron, 211 Bryant Space Sci Ctr,POB 112055, Gainesville, FL 32611 USA.
EM jpaty@mail.ustc.edu.cn
RI Gonzalez Hernandez, Jonay I./L-3556-2014; Ogando, Ricardo/A-1747-2010;
OI Gonzalez Hernandez, Jonay I./0000-0002-0264-7356; Ogando,
Ricardo/0000-0003-2120-1154; Fleming, Scott/0000-0003-0556-027X;
Eastman, Jason/0000-0003-3773-5142; /0000-0002-0802-9145; Pepper,
Joshua/0000-0002-3827-8417
FU W. M. Keck Foundation; NSF [AST-0705139]; SDSS-III consortium; NASA
[NNX07AP14G]; University of Florida; Alfred P. Sloan Foundation;
National Science Foundation; U.S. Department of Energy; University of
Arizona; Brazilian Participation Group; University of Cambridge; French
Participation Group; German Participation Group; Michigan
State/NotreDame/JINA Participation Group; Johns Hopkins University;
Lawrence Berkeley National Laboratory; Max Planck Institute for
Astrophysics; New Mexico State University; New York University; Ohio
State University; University of Portsmouth; Princeton University;
University of Tokyo; University of Utah; Vanderbilt University;
University of Virginia; University of Washington; Yale University
FX Funding for the MARVELS multi-object Doppler instrument was provided by
the W. M. Keck Foundation and NSF with grant AST-0705139. The MARVELS
survey was partially funded by the SDSS-III consortium, NSF grant
AST-0705139, NASA with grant NNX07AP14G and the University of Florida.
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. 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, University of Cambridge, University of Florida, the
French Participation Group, the German Participation Group, the Michigan
State/NotreDame/JINA Participation Group, Johns Hopkins University,
Lawrence Berkeley National Laboratory, Max Planck Institute for
Astrophysics, New Mexico State University, New York University, the Ohio
State University, University of Portsmouth, Princeton University,
University of Tokyo, the University of Utah, Vanderbilt University,
University of Virginia, University of Washington, and Yale University.
NR 90
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2013
VL 146
IS 3
AR 65
DI 10.1088/0004-6256/146/3/65
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 203OO
UT WOS:000323302700022
ER
PT J
AU Meixner, M
Panuzzo, P
Roman-Duval, J
Engelbracht, C
Babler, B
Seale, J
Hony, S
Montiel, E
Sauvage, M
Gordon, K
Misselt, K
Okumura, K
Chanial, P
Beck, T
Bernard, JP
Bolatto, A
Bot, C
Boyer, ML
Carlson, LR
Clayton, GC
Chen, CHR
Cormier, D
Fukui, Y
Galametz, M
Galliano, F
Hora, JL
Hughes, A
Indebetouw, R
Israel, FP
Kawamura, A
Kemper, F
Kim, S
Kwon, E
Lebouteiller, V
Li, A
Long, KS
Madden, SC
Matsuura, M
Muller, E
Oliveira, JM
Onishi, T
Otsuka, M
Paradis, D
Poglitsch, A
Reach, WT
Robitaille, TP
Rubio, M
Sargent, B
Sewilo, M
Skibba, R
Smith, LJ
Srinivasan, S
Tielens, AGGM
van Loon, JT
Whitney, B
AF Meixner, M.
Panuzzo, P.
Roman-Duval, J.
Engelbracht, C.
Babler, B.
Seale, J.
Hony, S.
Montiel, E.
Sauvage, M.
Gordon, K.
Misselt, K.
Okumura, K.
Chanial, P.
Beck, T.
Bernard, J. -P.
Bolatto, A.
Bot, C.
Boyer, M. L.
Carlson, L. R.
Clayton, G. C.
Chen, C. -H. R.
Cormier, D.
Fukui, Y.
Galametz, M.
Galliano, F.
Hora, J. L.
Hughes, A.
Indebetouw, R.
Israel, F. P.
Kawamura, A.
Kemper, F.
Kim, S.
Kwon, E.
Lebouteiller, V.
Li, A.
Long, K. S.
Madden, S. C.
Matsuura, M.
Muller, E.
Oliveira, J. M.
Onishi, T.
Otsuka, M.
Paradis, D.
Poglitsch, A.
Reach, W. T.
Robitaille, T. P.
Rubio, M.
Sargent, B.
Sewilo, M.
Skibba, R.
Smith, L. J.
Srinivasan, S.
Tielens, A. G. G. M.
van Loon, J. Th.
Whitney, B.
TI THE HERSCHEL INVENTORY OF THE AGENTS OF GALAXY EVOLUTION IN THE
MAGELLANIC CLOUDS, A HERSCHEL OPEN TIME KEY PROGRAM
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE catalogs; dust, extinction; infrared: galaxies; Magellanic Clouds;
submillimeter: general; surveys
ID STAR-FORMATION HISTORY; YOUNG STELLAR OBJECTS; III PHOTOMETRIC MAPS; LOW
METALLICITY; SPITZER SURVEY; MOLECULAR CLOUDS; EVOLVED STARS; INFRARED
OBSERVATIONS; APERTURE SYNTHESIS; EXCESS EMISSION
AB We present an overview of the HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE) in the Magellanic Clouds project, which is a Herschel Space Observatory open time key program. We mapped the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) at 100, 160, 250, 350, and 500 mu m with the Spectral and Photometric Imaging Receiver (SPIRE) and Photodetector Array Camera and Spectrometer (PACS) instruments on board Herschel using the SPIRE/PACS parallel mode. The overriding science goal of HERITAGE is to study the life cycle of matter as traced by dust in the LMC and SMC. The far-infrared and submillimeter emission is an effective tracer of the interstellar medium (ISM) dust, the most deeply embedded young stellar objects (YSOs), and the dust ejected by the most massive stars. We describe in detail the data processing, particularly for the PACS data, which required some custom steps because of the large angular extent of a single observational unit and overall the large amount of data to be processed as an ensemble. We report total global fluxes for the LMC and SMC and demonstrate their agreement with measurements by prior missions. The HERITAGE maps of the LMC and SMC are dominated by the ISM dust emission and bear most resemblance to the tracers of ISM gas rather than the stellar content of the galaxies. We describe the point source extraction processing and the criteria used to establish a catalog for each waveband for the HERITAGE program. The 250 mu m band is the most sensitive and the source catalogs for this band have similar to 25,000 objects for the LMC and similar to 5500 objects for the SMC. These data enable studies of ISM dust properties, submillimeter excess dust emission, dust-to-gas ratio, Class 0 YSO candidates, dusty massive evolved stars, supernova remnants (including SN1987A), H II regions, and dust evolution in the LMC and SMC. All images and catalogs are delivered to the Herschel Science Center as part of the community support aspects of the project. These HERITAGE images and catalogs provide an excellent basis for future research and follow up with other facilities.
C1 [Meixner, M.; Roman-Duval, J.; Seale, J.; Gordon, K.; Beck, T.; Boyer, M. L.; Long, K. S.; Sargent, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Meixner, M.; Sewilo, M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Panuzzo, P.; Hony, S.; Sauvage, M.; Okumura, K.; Chanial, P.; Cormier, D.; Galliano, F.; Lebouteiller, V.; Madden, S. C.] CEA, Irfu SAp, Lab AIM, F-91191 Gif Sur Yvette, France.
[Panuzzo, P.] Observ Paris, CNRS, Lab GEPI, F-92195 Meudon, France.
[Engelbracht, C.; Montiel, E.; Misselt, K.; Skibba, R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Engelbracht, C.] Raytheon Co, Tucson, AZ 85756 USA.
[Babler, B.; Whitney, B.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Montiel, E.; Clayton, G. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Bernard, J. -P.; Paradis, D.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Bernard, J. -P.; Paradis, D.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Bolatto, A.] Univ Maryland, Dept Astron, Lab Millimeter Wave Astron, College Pk, MD 20742 USA.
[Bot, C.] Univ Strasbourg, Observ Astron Strasbourg, F-67000 Strasbourg, France.
[Bot, C.] CNRS, Observ Astron Strasbourg, UMR7550, F-67000 Strasbourg, France.
[Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Boyer, M. L.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Carlson, L. R.; Israel, F. P.; Tielens, A. G. G. M.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
[Chen, C. -H. R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Fukui, Y.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Galametz, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Hora, J. L.] Harvard Univ, Ctr Astrophys, Cambridge, MA 02138 USA.
[Hughes, A.; Robitaille, T. P.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Kawamura, A.; Muller, E.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Kemper, F.; Otsuka, M.; Srinivasan, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Kim, S.; Kwon, E.] Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea.
[Li, A.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
[Matsuura, M.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Oliveira, J. M.; van Loon, J. Th.] Keele Univ, Lennard Jones Labs, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England.
[Onishi, T.] Osaka Prefecture Univ, Dept Phys Sci, Sakai, Osaka 5998531, Japan.
[Poglitsch, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA.
[Rubio, M.] Univ Chile, Dept Astron, Santiago, Chile.
[Sargent, B.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
[Sargent, B.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA.
[Smith, L. J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Smith, L. J.] European Space Agcy, Baltimore, MD 21218 USA.
[Srinivasan, S.] Inst Astrophys, UPMC CNRS, UMR7095, F-75014 Paris, France.
RP Meixner, M (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM meixner@stsci.edu
RI Kemper, Francisca/D-8688-2011; Rubio, Monica/J-3384-2016;
OI Kemper, Francisca/0000-0003-2743-8240; Bot,
Caroline/0000-0001-6118-2985; Babler, Brian/0000-0002-6984-5752;
Lebouteiller, Vianney/0000-0002-7716-6223; Reach,
William/0000-0001-8362-4094; Robitaille, Thomas/0000-0002-8642-1329
FU NASA Herschel Science Center, JPL [1381522, 1381650, 1350371]; FONDECYT
[1080335]; FONDAP [15010003]; National Science Council
[NSC100-2112-M-001-023-MY3]; European Space Agency (ESA); Herschel
Science Center; NASA Herschel Science Center; PACS; SPIRE Instrument
Control Centers
FX We acknowledge financial support from the NASA Herschel Science Center,
JPL contract Nos. 1381522 and 1381650. M. R. is supported by FONDECYT
No1080335 and FONDAP No15010003. F. K. acknowledges support from the
National Science Council in the form of grant NSC100-2112-M-001-023-MY3.
R. A. S. acknowledges financial support from the NASA Herschel Science
Center, JPL contract No. 1350371. We are thankful for the contributions
and support from the European Space Agency (ESA), the PACS and SPIRE
teams, the Herschel Science Center (esp. L. Conversi) and the NASA
Herschel Science Center (esp. A. Barbar and R. Paladini), and the PACS
and SPIRE Instrument Control Centers (esp. George Bendo), without which
none of this work would be possible.
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JI Astron. J.
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SC Astronomy & Astrophysics
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UT WOS:000323302700019
ER
PT J
AU Sabbi, E
Anderson, J
Lennon, DJ
van der Marel, RP
Aloisi, A
Boyer, ML
Cignoni, M
de Marchi, G
de Mink, SE
Evans, CJ
Gallagher, JS
Gordon, K
Gouliermis, DA
Grebel, EK
Koekemoer, AM
Larsen, SS
Panagia, N
Ryon, JE
Smith, LJ
Tosi, M
Zaritsky, D
AF Sabbi, E.
Anderson, J.
Lennon, D. J.
van der Marel, R. P.
Aloisi, A.
Boyer, M. L.
Cignoni, M.
de Marchi, G.
de Mink, S. E.
Evans, C. J.
Gallagher, J. S., III
Gordon, K.
Gouliermis, D. A.
Grebel, E. K.
Koekemoer, A. M.
Larsen, S. S.
Panagia, N.
Ryon, J. E.
Smith, L. J.
Tosi, M.
Zaritsky, D.
TI HUBBLE TARANTULA TREASURY PROJECT: UNRAVELING TARANTULA'S WEB. I.
OBSERVATIONAL OVERVIEW AND FIRST RESULTS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: star clusters: individual (30 Doradus); Magellanic Clouds;
stars: formation; stars: imaging; stars: pre-main sequence
ID LARGE-MAGELLANIC-CLOUD; 30 DORADUS NEBULA; YOUNG STELLAR POPULATIONS;
STAR-FORMATION HISTORY; INITIAL MASS FUNCTION; LYMAN BREAK GALAXIES;
ALL-SKY SURVEY; DWARF GALAXIES; IRREGULAR GALAXIES; INTERMEDIATE-MASS
AB The Hubble Tarantula Treasury Project (HTTP) is an ongoing panchromatic imaging survey of stellar populations in the Tarantula Nebula in the Large Magellanic Cloud that reaches into the sub-solar mass regime (<0.5 M-circle dot). HTTP utilizes the capability of the Hubble Space Telescope to operate the Advanced Camera for Surveys and the Wide Field Camera 3 in parallel to study this remarkable region in the near-ultraviolet, optical, and near-infrared spectral regions, including narrow-band H alpha images. The combination of all these bands provides a unique multi-band view. The resulting maps of the stellar content of the Tarantula Nebula within its main body provide the basis for investigations of star formation in an environment resembling the extreme conditions found in starburst galaxies and in the early universe. Access to detailed properties of individual stars allows us to begin to reconstruct the temporal and spatial evolution of the stellar skeleton of the Tarantula Nebula over space and time on a sub-parsec scale. In this first paper we describe the observing strategy, the photometric techniques, and the upcoming data products from this survey and present preliminary results obtained from the analysis of the initial set of near-infrared observations.
C1 [Sabbi, E.; Anderson, J.; van der Marel, R. P.; Aloisi, A.; de Mink, S. E.; Gordon, K.; Koekemoer, A. M.; Panagia, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Lennon, D. J.] ESA, European Space Astron Ctr, E-28691 Madrid, Spain.
[Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Boyer, M. L.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Cignoni, M.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Cignoni, M.; Tosi, M.] Osservatorio Astron Bologna, Ist Nazl Astrofis, I-40127 Bologna, Italy.
[de Marchi, G.] European Space Agcy, Dept Space Sci, NL-2200 AG Noordwijk, Netherlands.
[de Mink, S. E.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Evans, C. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Gallagher, J. S., III; Ryon, J. E.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Gouliermis, D. A.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany.
[Grebel, E. K.] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany.
[Larsen, S. S.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Panagia, N.] Osserv Astrofis Catania, Ist Nazl Astrofis, I-95123 Catania, Italy.
[Smith, L. J.] ESA, STScI, Baltimore, MD 21218 USA.
[Zaritsky, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Sabbi, E (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM sabbi@stsci.edu
RI Tosi, Monica/O-9377-2015; Cignoni, Michele/J-9365-2016;
OI Tosi, Monica/0000-0002-0986-4759; Cignoni, Michele/0000-0001-6291-6813;
de Mink, Selma/0000-0001-9336-2825; Lennon, Daniel/0000-0003-3063-4867;
Gouliermis, Dimitrios/0000-0002-2763-0075; /0000-0002-1891-3794;
Koekemoer, Anton/0000-0002-6610-2048
FU NASA through Space Telescope Science Institute [GO-12499, GO-12939];
NASA [NAS 5-26555]; Collaborative Research Center "The Milky Way System"
of the German Research Foundation (DFG) [SFB 881]; German Research
Foundation (DFG) [GO 1659/3-1]; NASA through Hubble Fellowship
[HST-HF-51270.01-A]; Space Telescope Science Institute; [ASI
I009/10/0]; [PRIN-INAF-2010]; [PRIN-MIUR-2010-11]
FX The authors are grateful to Zolt Levay for his work on the images shown
in Figures 1 and 3. M. T. and M. C. have been partially funded by
contracts ASI I009/10/0, PRIN-INAF-2010 and PRIN-MIUR-2010-11. Support
for programs GO-12499 and GO-12939 was provided by NASA through grants
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. E. K. G. acknowledges support from the
Collaborative Research Center "The Milky Way System" (SFB 881) of the
German Research Foundation (DFG), particularly by subproject B5. D. A.
G. kindly acknowledges financial support by the German Research
Foundation (DFG) through grant GO 1659/3-1. S.d.M. acknowledges support
by NASA through Hubble Fellowship grant HST-HF-51270.01-A 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.
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SC Astronomy & Astrophysics
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ER
PT J
AU Barnes, JW
van Eyken, JC
Jackson, BK
Ciardi, DR
Fortney, JJ
AF Barnes, Jason W.
van Eyken, Julian C.
Jackson, Brian K.
Ciardi, David R.
Fortney, Jonathan J.
TI MEASUREMENT OF SPIN-ORBIT MISALIGNMENT AND NODAL PRECESSION FOR THE
PLANET AROUND PRE-MAIN-SEQUENCE STAR PTFO 8-8695 FROM GRAVITY DARKENING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; planetary systems; stars: individual (PTFO 8-8695);
techniques: photometric
ID TRANSITING EXTRASOLAR PLANETS; RAPIDLY ROTATING STARS; TIME-SERIES
PHOTOMETRY; HOT-JUPITER; LIGHT CURVES; OBLIQUITY; SYSTEM; BINARY; MASS;
PERTURBATIONS
AB PTFO 8-8695b represents the first transiting exoplanet candidate orbiting a pre-main-sequence star (van Eyken et al. 2012, ApJ, 755, 42). We find that the unusual lightcurve shapes of PTFO 8-8695 can be explained by transits of a planet across an oblate, gravity-darkened stellar disk. We develop a theoretical framework for understanding precession of a planetary orbit's ascending node for the case when the stellar rotational angular momentum and the planetary orbital angular momentum are comparable in magnitude. We then implement those ideas to simultaneously and self-consistently fit two separate lightcurves observed in 2009 December and 2010 December. Our two self-consistent fits yield M-p = 3.0 M-Jup and M-p = 3.6 M-Jup for assumed stellar masses of M-* = 0.34 M-circle dot and M-* = 0.44 M-circle dot respectively. The two fits have precession periods of 293 days and 581 days. These mass determinations (consistent with previous upper limits) along with the strength of the gravity-darkened precessing model together validate PTFO 8-8695b as just the second hot Jupiter known to orbit an M-dwarf. Our fits show a high degree of spin-orbit misalignment in the PTFO 8-8695 system: 69 degrees +/- 2 degrees or 73 degrees.1 +/- 0 degrees.5, in the two cases. The large misalignment is consistent with the hypothesis that planets become hot Jupiters with random orbital plane alignments early in a system's lifetime. We predict that as a result of the highly misaligned, precessing system, the transits should disappear for months at a time over the course of the system's precession period. The precessing, gravity-darkened model also predicts other observable effects: changing orbit inclination that could be detected by radial velocity observations, changing stellar inclination that would manifest as varying v sin i, changing projected spin-orbit alignment that could be seen by the Rossiter-McLaughlin effect, changing transit shapes over the course of the precession, and differing lightcurves as a function of wavelength. Our measured planet radii of 1.64 R-Jup and 1.68 R-Jup in each case are consistent with a young, hydrogen-dominated planet that results from a "hot-start" formation mechanism.
C1 [Barnes, Jason W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
[van Eyken, Julian C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Jackson, Brian K.] DTM, Carnegie Inst Washington, Washington, DC 20015 USA.
[Ciardi, David R.] NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
RP Barnes, JW (reprint author), Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
EM jwbarnes@uidaho.edu
RI Barnes, Jason/B-1284-2009;
OI Barnes, Jason/0000-0002-7755-3530; Fortney,
Jonathan/0000-0002-9843-4354; Ciardi, David/0000-0002-5741-3047
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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UT WOS:000323426700053
ER
PT J
AU Boyer, ML
Girardi, L
Marigo, P
Williams, BF
Aringer, B
Nowotny, W
Rosenfield, P
Dorman, CE
Guhathakurta, P
Dalcanton, JJ
Melbourne, JL
Olsen, KAG
Weisz, DR
AF Boyer, M. L.
Girardi, L.
Marigo, P.
Williams, B. F.
Aringer, B.
Nowotny, W.
Rosenfield, P.
Dorman, C. E.
Guhathakurta, P.
Dalcanton, J. J.
Melbourne, J. L.
Olsen, K. A. G.
Weisz, D. R.
TI IS THERE A METALLICITY CEILING TO FORM CARBON STARS?-A NOVEL TECHNIQUE
REVEALS A SCARCITY OF C STARS IN THE INNER M31 DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M31); stars: AGB and post-AGB; stars: carbon;
stars: late-type
ID ASYMPTOTIC GIANT BRANCH; SMALL-MAGELLANIC-CLOUD; NEAR-INFRARED
IDENTIFICATION; HIGH-REDSHIFT GALAXIES; AGB-STARS; LOCAL GROUP; STELLAR
POPULATIONS; TP-AGB; SYNTHETIC PHOTOMETRY; RED SUPERGIANTS
AB We use medium-band near-infrared (NIR) Hubble Space Telescope WFC3 photometry with model NIR spectra of asymptotic giant branch (AGB) stars to develop a new tool for efficiently distinguishing carbon-rich (C-type) AGB stars from oxygen-rich (M-type) AGB stars in galaxies at the edge of and outside the Local Group. We present the results of a test of this method on a region of the inner disk of M31, where we find a surprising lack of C stars, contrary to the findings of previous C star searches in other regions of M31. We find only one candidate C star (plus up to six additional, less certain C star candidates), resulting in an extremely low ratio of C to M stars (C/M = (3.3(-0.1)(+20)) x 10(-4)) that is one to two orders of magnitude lower than other C/M estimates in M31. The low C/M ratio is likely due to the high metallicity in this region which impedes stars from achieving C/O > 1 in their atmospheres. These observations provide stringent constraints to evolutionary models of metal-rich AGB stars and suggest that there is a metallicity threshold above which M stars are unable to make the transition to C stars, dramatically affecting AGB mass loss and dust production and, consequently, the observed global properties of metal-rich galaxies.
C1 [Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Boyer, M. L.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Girardi, L.] Osservatorio Astron Padova INAF, I-35122 Padua, Italy.
[Marigo, P.] Univ Padua, Dept Phys & Astron G Galilei, I-35122 Padua, Italy.
[Williams, B. F.; Rosenfield, P.; Dalcanton, J. J.; Weisz, D. R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Aringer, B.; Nowotny, W.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria.
[Dorman, C. E.; Guhathakurta, P.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Melbourne, J. L.] CALTECH, Caltech Opt Observ, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Olsen, K. A. G.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RP Boyer, ML (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
EM martha.boyer@nasa.gov
FU NASA Postdoctoral Program at the Goddard Space Flight Center; NASA
[NAS5-26555]; NASA through HST from the STScI [GO-12862, GO-12055];
University of Padova [CPDA125588/12]; Austrian Science Fund (FWF)
[P21988-N16]
FX We thank the referee, Jacco van Loon, for thoughtful comments that
improved the manuscript and helped to clarify important issues. This
work was supported by the NASA Postdoctoral Program at the Goddard Space
Flight Center, administered by ORAU through a contract with NASA and by
NASA through HST grant numbers GO-12862 and GO-12055 from the STScI,
which is operated by AURA, Inc., under NASA contract NAS5-26555. P.M.
and L.G. acknowledge support from Progetto di Ateneo 2012, University of
Padova, ID: CPDA125588/12. This research was funded in part by the
Austrian Science Fund (FWF): P21988-N16.
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ER
PT J
AU Guennou, C
Auchere, F
Klimchuk, JA
Bocchialini, K
Parenti, S
AF Guennou, C.
Auchere, F.
Klimchuk, J. A.
Bocchialini, K.
Parenti, S.
TI CAN THE DIFFERENTIAL EMISSION MEASURE CONSTRAIN THE TIMESCALE OF ENERGY
DEPOSITION IN THE CORONA?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE plasmas; Sun: corona; Sun: UV radiation; techniques: spectroscopic
ID EXTREME-ULTRAVIOLET-SPECTRA; ACTIVE-REGION CORES; SOLAR PLASMAS.
APPLICATION; MEASURE DISTRIBUTIONS; SPECTROSCOPIC DIAGNOSTICS;
FUNDAMENTAL LIMITATIONS; LOOPS OBSERVATIONS; ATOMIC DATABASE;
TIME-DEPENDENCE; LINE SPECTRA
AB In this paper, the ability of the Hinode/EIS instrument to detect radiative signatures of coronal heating is investigated. Recent observational studies of active region cores suggest that both the low and high frequency heating mechanisms are consistent with observations. Distinguishing between these possibilities is important for identifying the physical mechanism(s) of the heating. The differential emission measure (DEM) tool is one diagnostic that allows us to make this distinction, through the amplitude of the DEM slope coolward of the coronal peak. It is therefore crucial to understand the uncertainties associated with these measurements. Using proper estimations of the uncertainties involved in the problem of DEM inversion, we derive confidence levels on the observed DEM slope. Results show that the uncertainty in the slope reconstruction strongly depends on the number of lines constraining the slope. Typical uncertainty is estimated to be about +/- 1.0 in the more favorable cases.
C1 [Guennou, C.; Auchere, F.; Bocchialini, K.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Parenti, S.] Royal Observ Belgium, B-1180 Brussels, Belgium.
RP Guennou, C (reprint author), Univ Paris 11, CNRS, Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France.
EM chloe.guennou@ias.u-psud.fr
RI Klimchuk, James/D-1041-2012;
OI Klimchuk, James/0000-0003-2255-0305; Auchere,
Frederic/0000-0003-0972-7022
FU Belgian Federal Science Policy Office; Institut d'Astrophysique Spatiale
(IAS); Royal Observatory of Belgium; NASA
FX S.P. acknowledges the support from the Belgian Federal Science Policy
Office through the international cooperation programs and the ESA-PRODEX
program and the support of the Institut d'Astrophysique Spatiale (IAS).
F.A. acknowledges the support of the Royal Observatory of Belgium. The
work of J.A.K. was supported by the NASA Supporting Research and
Technology Program. The authors would like to thank G. Del Zanna, H.
Warren, G. Doschek, M. Laming, E. Landi, H. Mason, J. Schmelz, and P.
Young for fruitful discussions and comments about atomic physics
uncertainties. Discussions with H. Mason, H. Warren, and P. Testa at the
second meeting of the Bradshaw/Mason International Space Science
Institute Team were also very helpful.
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EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
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SC Astronomy & Astrophysics
GA 205FA
UT WOS:000323426700031
ER
PT J
AU Kanner, J
Baker, J
Blackburn, L
Camp, J
Mooley, K
Mushotzky, R
Ptak, A
AF Kanner, Jonah
Baker, John
Blackburn, Lindy
Camp, Jordan
Mooley, Kunal
Mushotzky, Richard
Ptak, Andy
TI X-RAY TRANSIENTS IN THE ADVANCED LIGO/VIRGO HORIZON
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: nuclei; gravitational waves; surveys; X-rays: general
ID NEWTON SLEW SURVEY; ALL-SKY SURVEY; GRAVITATIONAL-WAVE BURSTS; TIDAL
DISRUPTION EVENT; FOLLOW-UP OBSERVATIONS; NEUTRON-STAR BINARIES; MASSIVE
BLACK-HOLE; XMM-NEWTON; ELECTROMAGNETIC COUNTERPARTS; ORPHAN AFTERGLOWS
AB Advanced LIGO and Advanced Virgo will be all-sky monitors for merging compact objects within a few hundred megaparsecs. Finding the electromagnetic counterparts to these events will require an understanding of the transient sky at low redshift (z < 0.1). We performed a systematic search for extragalactic, low redshift, transient events in the XMM-Newton Slew Survey. In a flux limited sample, we found that highly variable objects comprised 10% of the sample, and that of these, 10% were spatially coincident with cataloged optical galaxies. This led to 4 x 10(-4) transients per square degree above a flux threshold of 3x10(-12) erg cm(-2) s(-1) (0.2-2 keV) which might be confused with LIGO/Virgo counterparts. This represents the first extragalactic measurement of the soft X-ray transient rate within the Advanced LIGO/Virgo horizon. Our search revealed six objects that were spatially coincident with previously cataloged galaxies, lacked evidence for optical active galactic nuclei, displayed high luminosities similar to 10(43) erg s(-1), and varied in flux by more than a factor of 10 when compared with the ROSAT All-Sky Survey. At least four of these displayed properties consistent with previously observed tidal disruption events.
C1 [Kanner, Jonah] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Kanner, Jonah; Baker, John; Blackburn, Lindy; Camp, Jordan; Mushotzky, Richard; Ptak, Andy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mooley, Kunal] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Mushotzky, Richard] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Kanner, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
EM jonah.kanner@ligo.org
OI Kanner, Jonah/0000-0001-8115-0577
FU NASA; National Aeronautics and Space Administration; Alfred P. Sloan
Foundation; National Science Foundation; U.S. Department of Energy;
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; Johns Hopkins University; Joint
Institute for Nuclear Astrophysics; Kavli Institute for Particle
Astrophysics and Cosmology; 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
FX The authors are grateful for helpful discussions with Suvi Gezari,
Judith Racusin, Brennan Hughey, Tracy Huard, and Sjoert van Velzan. We
thank the anonymous referee for helpful comments. J.K. and L. B. were
supported by appointments to the NASA Postdoctoral Program at GSFC,
administered by Oak Ridge Associated Universities through a contract
with NASA. K. M. would like to thank Branimir Sesar, Eric Bellm, and Yi
Cao for help obtaining the P200 spectra, and Assaf Horesh for work with
the Keck Observatory.; 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. This research has made
use of data obtained from the High Energy Astrophysics Science Archive
Research Center (HEASARC), provided by NASA's Goddard Space Flight
Center.; 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/. 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.
NR 74
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2013
VL 774
IS 1
AR 63
DI 10.1088/0004-637X/774/1/63
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205FA
UT WOS:000323426700063
ER
PT J
AU Kuzuhara, M
Tamura, M
Kudo, T
Janson, M
Kandori, R
Brandt, TD
Thalmann, C
Spiegel, D
Biller, B
Carson, J
Hori, Y
Suzuki, R
Burrows, A
Henning, T
Turner, EL
McElwain, MW
Moro-Martin, A
Suenaga, T
Takahashi, YH
Kwon, J
Lucas, P
Abe, L
Brandner, W
Egner, S
Feldt, M
Fujiwara, H
Goto, M
Grady, CA
Guyon, O
Hashimoto, J
Hayano, Y
Hayashi, M
Hayashi, SS
Hodapp, KW
Ishii, M
Iye, M
Knapp, GR
Matsuo, T
Mayama, S
Miyama, S
Morino, JI
Nishikawa, J
Nishimura, T
Kotani, T
Kusakabe, N
Pyo, TS
Serabyn, E
Suto, H
Takami, M
Takato, N
Terada, H
Tomono, D
Watanabe, M
Wisniewski, JP
Yamada, T
Takami, H
Usuda, T
AF Kuzuhara, M.
Tamura, M.
Kudo, T.
Janson, M.
Kandori, R.
Brandt, T. D.
Thalmann, C.
Spiegel, D.
Biller, B.
Carson, J.
Hori, Y.
Suzuki, R.
Burrows, A.
Henning, T.
Turner, E. L.
McElwain, M. W.
Moro-Martin, A.
Suenaga, T.
Takahashi, Y. H.
Kwon, J.
Lucas, P.
Abe, L.
Brandner, W.
Egner, S.
Feldt, M.
Fujiwara, H.
Goto, M.
Grady, C. A.
Guyon, O.
Hashimoto, J.
Hayano, Y.
Hayashi, M.
Hayashi, S. S.
Hodapp, K. W.
Ishii, M.
Iye, M.
Knapp, G. R.
Matsuo, T.
Mayama, S.
Miyama, S.
Morino, J-I.
Nishikawa, J.
Nishimura, T.
Kotani, T.
Kusakabe, N.
Pyo, T-S.
Serabyn, E.
Suto, H.
Takami, M.
Takato, N.
Terada, H.
Tomono, D.
Watanabe, M.
Wisniewski, J. P.
Yamada, T.
Takami, H.
Usuda, T.
TI DIRECT IMAGING OF A COLD JOVIAN EXOPLANET IN ORBIT AROUND THE SUN-LIKE
STAR GJ 504
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: formation; stars: individual (GJ 504)
ID MAIN-SEQUENCE STARS; EXTRASOLAR GIANT PLANETS; SOLAR-TYPE STARS; HR 8799
PLANETS; EDGE-ON DISK; BROWN DWARFS; STELLAR ROTATION; FOMALHAUT B;
GRAVITATIONAL-INSTABILITY; MODEL ATMOSPHERES
AB Several exoplanets have recently been imaged at wide separations of > 10 AU from their parent stars. These span a limited range of ages (<50 Myr) and atmospheric properties, with temperatures of 800-1800 K and very red colors (J - H > 0.5 mag), implying thick cloud covers. Furthermore, substantial model uncertainties exist at these young ages due to the unknown initial conditions at formation, which can lead to an order of magnitude of uncertainty in the modeled planet mass. Here, we report the direct-imaging discovery of a Jovian exoplanet around the Sun-like star GJ 504, detected as part of the SEEDS survey. The system is older than all other known directly imaged planets; as a result, its estimated mass remains in the planetary regime independent of uncertainties related to choices of initial conditions in the exoplanet modeling. Using the most common exoplanet cooling model, and given the system age of 160(-60)(+350) Myr, GJ 504b has an estimated mass of 4(-1.0)(+4.5) Jupiter masses, among the lowest of directly imaged planets. Its projected separation of 43.5 AU exceeds the typical outer boundary of similar to 30 AU predicted for the core accretion mechanism. GJ 504b is also significantly cooler (510(-20)(+30) K) and has a bluer color (J - H = -0.23 mag) than previously imaged exoplanets, suggesting a largely cloud-free atmosphere accessible to spectroscopic characterization. Thus, it has the potential of providing novel insights into the origins of giant planets as well as their atmospheric properties.
C1 [Kuzuhara, M.] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan.
[Kuzuhara, M.; Tamura, M.; Kandori, R.; Hori, Y.; Suzuki, R.; Takahashi, Y. H.; Kwon, J.; Hayashi, M.; Iye, M.; Morino, J-I.; Nishikawa, J.; Kotani, T.; Kusakabe, N.; Suto, H.; Takami, H.; Usuda, T.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Kuzuhara, M.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Tamura, M.; Kwon, J.; Nishikawa, J.] Grad Univ Adv Studies, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
[Tamura, M.; Takahashi, Y. H.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Kudo, T.; Suenaga, T.; Egner, S.; Fujiwara, H.; Guyon, O.; Hayano, Y.; Hayashi, S. S.; Ishii, M.; Nishimura, T.; Pyo, T-S.; Takato, N.; Terada, H.; Tomono, D.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Janson, M.; Brandt, T. D.; Spiegel, D.; Burrows, A.; Turner, E. L.; Moro-Martin, A.; Knapp, G. R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Spiegel, D.] Inst Adv Study, Princeton, NJ 08540 USA.
[Biller, B.; Henning, T.; Brandner, W.; Feldt, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Turner, E. L.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
[McElwain, M. W.; Grady, C. A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Moro-Martin, A.] CAB CSIC INTA, Dept Astrophys, E-28850 Madrid, Spain.
[Lucas, P.] Univ Hertfordshire, Ctr Astrophys, Hatfield AL10 9AB, Herts, England.
[Abe, L.] Univ Nice Sophia Antipolis, Lab Lagrange, UMR 7293, CNRS,Observatoire Cote Azur, F-06108 Nice 2, France.
[Goto, M.] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Grady, C. A.] Eureka Sci, Oakland, CA 96002 USA.
[Hashimoto, J.; Wisniewski, J. P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Mayama, S.] Grad Univ Adv Studies, Miura, Kanagawa 2400193, Japan.
[Miyama, S.] Hiroshima Univ, Higashihiroshima, Hiroshima 7398511, Japan.
[Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei, 10617, Taiwan.
[Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Kuzuhara, M (reprint author), Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
EM m.kuzuhara@nao.ac.jp
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
FU KAKENHI [22000005, 23103002]; WPI Initiative, MEXT, Japan; NSF AST
[1008440, 1009203, 1009314]; Global COE program "From the Earth to
Earths"; JSPS through the JSPS Research Fellowship for Young Scientists;
NASA
FX The authors thank Dr. I. N. Reid for discussions about age estimations
of main-sequence stars. In addition, the authors have benefited from
useful discussions with Drs. M. Ikoma, H. Nagahara, Y. Abe, S. Sugita,
and B. Sato. Furthermore, the authors thank David Lafreniere for
generously providing the source code for the LOCI algorithm. Our
referee's careful reading of the manuscript and excellent suggestions
have improved the quality of this paper. The help from Subaru Telescope
staff is greatly appreciated. This work is partly supported by KAKENHI
22000005 (M.T.), KAKENHI 23103002 (M.H.), WPI Initiative, MEXT, Japan
(E.L.T), NSF AST 1008440 (C.A.G), and NSF AST 1009203 (J.C.), and NSF
AST 1009314 (J.P.W.). Also, M.K. is partly supported by the Global COE
program "From the Earth to Earths." M.K., Y.H., Y.T., and J.K. are
financially supported by the JSPS through the JSPS Research Fellowship
for Young Scientists. Part of this work was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA. Finally, the authors 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.
NR 111
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2013
VL 774
IS 1
AR 11
DI 10.1088/0004-637X/774/1/11
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205FA
UT WOS:000323426700011
ER
PT J
AU McDonald, M
Benson, BA
Vikhlinin, A
Stalder, B
Bleem, LE
de Haan, T
Lin, HW
Aird, KA
Ashby, MLN
Bautz, MW
Bayliss, M
Bocquet, S
Brodwin, M
Carlstrom, JE
Chang, CL
Cho, HM
Clocchiatti, A
Crawford, TM
Crites, AT
Desai, S
Dobbs, MA
Dudley, JP
Foley, RJ
Forman, WR
George, EM
Gettings, D
Gladders, MD
Gonzalez, AH
Halverson, NW
High, FW
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Jones, C
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Liu, J
Lueker, M
Luong-Van, D
Mantz, A
Marrone, DP
McMahon, JJ
Mehl, J
Meyer, SS
Miller, ED
Mocanu, L
Mohr, JJ
Montroy, TE
Murray, SS
Nurgaliev, D
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Rest, A
Ruel, J
Ruhl, JE
Saliwanchik, BR
Saro, A
Sayre, JT
Schaffer, KK
Shirokoff, E
Song, J
Suhada, R
Spieler, HG
Stanford, SA
Staniszewski, Z
Stark, AA
Story, K
van Engelen, A
Vanderlinde, K
Vieira, JD
Williamson, R
Zahn, O
Zenteno, A
AF McDonald, M.
Benson, B. A.
Vikhlinin, A.
Stalder, B.
Bleem, L. E.
de Haan, T.
Lin, H. W.
Aird, K. A.
Ashby, M. L. N.
Bautz, M. W.
Bayliss, M.
Bocquet, S.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Cho, H. M.
Clocchiatti, A.
Crawford, T. M.
Crites, A. T.
Desai, S.
Dobbs, M. A.
Dudley, J. P.
Foley, R. J.
Forman, W. R.
George, E. M.
Gettings, D.
Gladders, M. D.
Gonzalez, A. H.
Halverson, N. W.
High, F. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hrubes, J. D.
Jones, C.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Liu, J.
Lueker, M.
Luong-Van, D.
Mantz, A.
Marrone, D. P.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Miller, E. D.
Mocanu, L.
Mohr, J. J.
Montroy, T. E.
Murray, S. S.
Nurgaliev, D.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Rest, A.
Ruel, J.
Ruhl, J. E.
Saliwanchik, B. R.
Saro, A.
Sayre, J. T.
Schaffer, K. K.
Shirokoff, E.
Song, J.
Suhada, R.
Spieler, H. G.
Stanford, S. A.
Staniszewski, Z.
Stark, A. A.
Story, K.
van Engelen, A.
Vanderlinde, K.
Vieira, J. D.
Williamson, R.
Zahn, O.
Zenteno, A.
TI THE GROWTH OF COOL CORES AND EVOLUTION OF COOLING PROPERTIES IN A SAMPLE
OF 83 GALAXY CLUSTERS AT 0.3 < z < 1.2 SELECTED FROM THE SPT-SZ SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE early universe; galaxies: clusters: general; galaxies: clusters:
intracluster medium; X-rays: galaxies: clusters
ID SOUTH-POLE TELESCOPE; ACTIVE GALACTIC NUCLEI; RAY LUMINOUS CLUSTERS;
COLD MOLECULAR GAS; 720 SQUARE DEGREES; STAR-FORMATION; FLOW CLUSTERS;
HIGH-REDSHIFT; INTRACLUSTER MEDIUM; PERSEUS CLUSTER
AB We present first results on the cooling properties derived from Chandra X-ray observations of 83 high-redshift (0.3 < z < 1.2) massive galaxy clusters selected by their Sunyaev-Zel'dovich signature in the South Pole Telescope data. We measure each cluster's central cooling time, central entropy, and mass deposition rate, and compare these properties to those for local cluster samples. We find no significant evolution from z similar to 0 to z similar to 1 in the distribution of these properties, suggesting that cooling in cluster cores is stable over long periods of time. We also find that the average cool core entropy profile in the inner similar to 100 kpc has not changed dramatically since z similar to 1, implying that feedback must be providing nearly constant energy injection to maintain the observed "entropy floor" at similar to 10 keV cm(2). While the cooling properties appear roughly constant over long periods of time, we observe strong evolution in the gas density profile, with the normalized central density (rho(g),(0)/rho(crit)) increasing by an order of magnitude from z similar to 1 to z similar to 0. When using metrics defined by the inner surface brightness profile of clusters, we find an apparent lack of classical, cuspy, cool-core clusters at z > 0.75, consistent with earlier reports for clusters at z > 0.5 using similar definitions. Our measurements indicate that cool cores have been steadily growing over the 8 Gyr spanned by our sample, consistent with a constant, similar to 150M(circle dot) yr(-1) cooling flow that is unable to cool below entropies of 10 keV cm(2) and, instead, accumulates in the cluster center. We estimate that cool cores began to
C1 [McDonald, M.; Bautz, M. W.; Miller, E. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mantz, A.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Vikhlinin, A.; Stalder, B.; Ashby, M. L. N.; Bayliss, M.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; van Engelen, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Lin, H. W.] Caddo Parish Magnet High Sch, Shrevport, LA 71101 USA.
[Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA.
[Bayliss, M.; Nurgaliev, D.; Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Suhada, R.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Univ, D-85748 Garching, Germany.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Chang, C. L.; Mehl, J.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Clocchiatti, A.] Pontificia Univ Catolica, Dept Astron & Astrosif, Santiago, Chile.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Gettings, D.; Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA.
[Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Lueker, M.; Padin, S.; Shirokoff, E.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA.
[Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA.
[Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
RP McDonald, M (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM mcdonald@space.mit.edu
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518;
Reichardt, Christian/0000-0003-2226-9169; Lin, Henry/0000-0003-2767-6142
FU NASA [HST-HF51308.01-A, 12800071, 12800088, 13800883]; Space Telescope
Science Institute; Association of Universities for Research in
Astronomy, Inc., for NASA [NAS 5-26555]; National Science Foundation
[ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli
Foundation; Gordon and Betty Moore Foundation; NSF [AST-1009012,
AST-1009649, MRI-0723073]; U.S. Department of Energy [DE-AC02-06CH11357]
FX M.M. acknowledges support by NASA through a Hubble Fellowship grant
HST-HF51308.01-A 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. The South Pole
Telescope program is supported by the National Science Foundation
through grant ANT-0638937. Partial support is also provided by the NSF
Physics Frontier Center grant PHY-0114422 to the Kavli Institute of
Cosmological Physics at the University of Chicago, the Kavli Foundation,
and the Gordon and Betty Moore Foundation. Support for X-ray analysis
was provided by NASA through Chandra Award Nos. 12800071, 12800088, and
13800883 issued by the Chandra X-Ray Observatory Center, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of NASA. Galaxy cluster research at Harvard is supported by NSF grant
AST-1009012 and at SAO in part by NSF grants AST-1009649 and
MRI-0723073. Argonne National Laboratory's work was supported under U.S.
Department of Energy contract DE-AC02-06CH11357.
NR 95
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U1 1
U2 12
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 SEP 1
PY 2013
VL 774
IS 1
AR UNSP 23
DI 10.1088/0004-637X/774/1/23
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205FA
UT WOS:000323426700023
ER
PT J
AU McGuire, BA
Carroll, PB
Loomis, RA
Blake, GA
Hollis, JM
Lovas, FJ
Jewell, PR
Remijan, AJ
AF McGuire, Brett A.
Carroll, P. Brandon
Loomis, Ryan A.
Blake, Geoffrey A.
Hollis, Jan M.
Lovas, Frank J.
Jewell, Philip R.
Remijan, Anthony J.
TI A SEARCH FOR l-C3H+ AND l-C3H IN Sgr B2(N), Sgr B2(OH), AND THE DARK
CLOUD TMC-1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: clouds; ISM: individual objects (Sagittarius B2(N),
Sagittarius B2(OH), TMC-1); ISM: molecules
ID LABORATORY MICROWAVE-SPECTRUM; LINE SURVEY; ASTRONOMICAL IDENTIFICATION;
VIBRATIONAL FREQUENCIES; SPECTROSCOPIC CONSTANTS; PRIMOS SURVEY; IRC
&10216; INTERSTELLAR; ION; GHZ
AB Pety et al. recently reported the detection of several transitions of an unknown carrier in the Horsehead PDR and attribute them to l-C3H+. Here, we have tested the predictive power of their fit by searching for, and identifying, the previously unobserved J = 1-0 and J = 2-1 transitions of the unknown carrier (B11244) toward Sgr B2(N) in data from the publicly available PRIMOS project. Also presented here are observations of the J = 6-5 and J = 7-6 transitions toward Sgr B2(N) and Sgr B2(OH) using the Barry E. Turner Legacy Survey and results from the Kaifu et al. survey of TMC-1. We calculate an excitation temperature and column density of B11244 of similar to 10 K and similar to 10(13) cm(-2) in Sgr B2(N) and similar to 79 K with an upper limit of <= 1.5 x 10(13) cm(-2) in Sgr B2(OH) and find trace evidence for the cation's presence in TMC-1. Finally, we present spectra of the neutral species in both Sgr B2(N) and TMC-1, and comment on the robustness of the assignment of the detected signals to l-C3H+.
C1 [McGuire, Brett A.; Carroll, P. Brandon; Blake, Geoffrey A.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
[Loomis, Ryan A.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA.
[Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Hollis, Jan M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lovas, Frank J.] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA.
[Jewell, Philip R.; Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
RP McGuire, BA (reprint author), CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
OI McGuire, Brett/0000-0003-1254-4817
FU NSF Graduate Research Fellowship
FX The authors are grateful to M. Ohishi for providing the observational
data toward TMC-1 and to the anonymous referee for very helpful
comments. B. A. M. gratefully acknowledges funding by an NSF Graduate
Research Fellowship. The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc.
NR 36
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U1 1
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2013
VL 774
IS 1
AR 56
DI 10.1088/0004-637X/774/1/56
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205FA
UT WOS:000323426700056
ER
PT J
AU Qiu, J
Sturrock, Z
Longcope, DW
Klimchuk, JA
Liu, WJ
AF Qiu, Jiong
Sturrock, Zoe
Longcope, Dana W.
Klimchuk, James A.
Liu, Wen-Juan
TI ULTRAVIOLET AND EXTREME-ULTRAVIOLET EMISSIONS AT THE FLARE FOOTPOINTS
OBSERVED BY ATMOSPHERE IMAGING ASSEMBLY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic reconnection; Sun: flares; Sun: UV radiation
ID HARD X-RAY; GENTLE CHROMOSPHERIC EVAPORATION; BRAGG CRYSTAL
SPECTROMETER; SOLAR-FLARE; IMPULSIVE PHASE; MULTIWAVELENGTH
OBSERVATIONS; MOMENTUM BALANCE; ATOMIC DATABASE; CORONAL LOOP;
RECONNECTION
AB A solar flare is composed of impulsive energy release events by magnetic reconnection, which forms and heats flare loops. Recent studies have revealed a two-phase evolution pattern of UV 1600 angstrom emission at the feet of these loops: a rapid pulse lasting for a few seconds to a few minutes, followed by a gradual decay on timescales of a few tens of minutes. Multiple band EUV observations by the Atmosphere Imaging Assembly further reveal very similar signatures. These two phases represent different but related signatures of an impulsive energy release in the corona. The rapid pulse is an immediate response of the lower atmosphere to an intense thermal conduction flux resulting from the sudden heating of the corona to high temperatures (we rule out energetic particles due to a lack of significant hard X-ray emission). The gradual phase is associated with the cooling of hot plasma that has been evaporated into the corona. The observed footpoint emission is again powered by thermal conduction (and enthalpy), but now during a period when approximate steady-state conditions are established in the loop. UV and EUV light curves of individual pixels may therefore be separated into contributions from two distinct physical mechanisms to shed light on the nature of energy transport in a flare. We demonstrate this technique using coordinated, spatially resolved observations of UV and EUV emissions from the footpoints of a C3.2 thermal flare.
C1 [Qiu, Jiong; Longcope, Dana W.; Liu, Wen-Juan] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
[Sturrock, Zoe] Univ St Andrews, Dept Appl Math, St Andrews KY16 9AJ, Fife, Scotland.
[Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Qiu, J (reprint author), Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
RI Liu, WenJuan/A-5069-2012; Klimchuk, James/D-1041-2012
OI Liu, WenJuan/0000-0001-9927-4471; Klimchuk, James/0000-0003-2255-0305
FU NSF grant [ATM-0748428]; NASA Supporting Research and Technology Program
FX We thank Dr. R. C. Canfield for illuminating us about the flare
energetics and lower-atmosphere heating. We thank the referee for a
careful reading of the manuscript and constructive comments that help
improve clarity of the paper. We acknowledge SDO for providing quality
observations. The work by J.Q. and W.L. is supported by NSF grant
ATM-0748428. Part of the work was conducted during the NSF REU Program
at Montana State University. D.W.L. acknowledges support by the NASA
Supporting Research and Technology Program. The work of J.A.K. was
supported by the NASA Supporting Research and Technology Program.
NR 64
TC 7
Z9 7
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 SEP 1
PY 2013
VL 774
IS 1
AR 14
DI 10.1088/0004-637X/774/1/14
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205FA
UT WOS:000323426700014
ER
PT J
AU Temim, T
Dwek, E
AF Temim, Tea
Dwek, Eli
TI THE IMPORTANCE OF PHYSICAL MODELS FOR DERIVING DUST MASSES AND GRAIN
SIZE DISTRIBUTIONS IN SUPERNOVA EJECTA. I. RADIATIVELY HEATED DUST IN
THE CRAB NEBULA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: ISM; ISM: individual objects (Crab Nebula);
ISM: supernova remnants; pulsars: individual (PSR B0531+21)
ID LARGE-MAGELLANIC-CLOUD; DIFFUSE INTERSTELLAR-MEDIUM;
SPITZER-SPACE-TELESCOPE; EARLY UNIVERSE; MASSIVE STARS;
PHOTOELECTRIC-EMISSION; CHEMICAL EVOLUTION; INFRARED-EMISSION; II
SUPERNOVAE; AGB STARS
AB Recent far-infrared (IR) observations of supernova remnants (SNRs) have revealed significantly large amounts of newly condensed dust in their ejecta, comparable to the total mass of available refractory elements. The dust masses derived from these observations assume that all the grains of a given species radiate at the same temperature, regardless of the dust heating mechanism or grain radius. In this paper, we derive the dust mass in the ejecta of the Crab Nebula, using a physical model for the heating and radiation from the dust. We adopt a power-law distribution of grain sizes and two different dust compositions (silicates and amorphous carbon), and calculate the heating rate of each dust grain by the radiation from the pulsar wind nebula. We find that the grains attain a continuous range of temperatures, depending on their size and composition. The total mass derived from the best-fit models to the observed IR spectrum is 0.019-0.13 M-circle dot, depending on the assumed grain composition. We find that the power-law size distribution of dust grains is characterized by a power-law index of 3.5-4.0 and a maximum grain size larger than 0.1 mu m. The grain sizes and composition are consistent with what is expected for dust grains formed in a Type IIP supernova (SN). Our derived dust mass is at least a factor of two less than the mass reported in previous studies of the Crab Nebula that assumed more simplified two-temperature models. These models also require a larger mass of refractory elements to be locked up in dust than was likely available in the ejecta. The results of this study show that a physical model resulting in a realistic distribution of dust temperatures can constrain the dust properties and affect the derived dust masses. Our study may also have important implications for deriving grain properties and mass estimates in other SNRs and for the ultimate question of whether SNe are major sources of dust in the Galactic interstellar medium and in external galaxies.
C1 [Temim, Tea; Dwek, Eli] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Temim, Tea] ORAU, Oak Ridge, TN 37831 USA.
RP Temim, T (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
EM tea.temim@nasa.gov
OI Temim, Tea/0000-0001-7380-3144
NR 66
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U1 0
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2013
VL 774
IS 1
AR 8
DI 10.1088/0004-637X/774/1/8
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205FA
UT WOS:000323426700008
ER
PT J
AU Deck, KM
Holman, MJ
Agol, E
Carter, JA
Lissauer, JJ
Ragozzine, D
Winn, JN
AF Deck, Katherine M.
Holman, Matthew J.
Agol, Eric
Carter, Joshua A.
Lissauer, Jack J.
Ragozzine, Darin
Winn, Joshua N.
TI RAPID DYNAMICAL CHAOS IN AN EXOPLANETARY SYSTEM (vol 755, pg L21, 2012)
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Correction
C1 [Deck, Katherine M.; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Deck, Katherine M.; Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Holman, Matthew J.; Carter, Joshua A.; Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Lissauer, Jack J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Deck, KM (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
NR 2
TC 0
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U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 1
PY 2013
VL 774
IS 1
AR L15
DI 10.1088/2041-8205/774/1/L15
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 208IV
UT WOS:000323672400015
ER
PT J
AU Gasper, JR
Kruse, GH
AF Gasper, Jason R.
Kruse, Gordon H.
TI Modeling of the spatial distribution of Pacific spiny dogfish (Squalus
suckleyi) in the Gulf of Alaska using generalized additive and
generalized linear models
SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES
LA English
DT Article
ID NORTH PACIFIC; ACANTHIAS; POPULATION; SHARK; CATCH; PARAMETER; PATTERNS
AB The Pacific spiny dogfish (Squalus suckleyi) is a common bycatch species in the Gulf of Alaska. Their spatial distribution is poorly understood, as most catch is discarded at sea. We analyzed spiny dogfish spatial distribution from fishery-dependent and -independent observations of longline gear between 1996 and 2008 using generalized additive and generalized linear models. Poisson, negative binomial, and quasi-Poisson error structures were investigated; the quasi-Poisson generalized additive model fit best. Models showed that spiny dogfish catches were concentrated east of Kodiak Island in waters <= 100 m deep. Results facilitate design of future spiny dogfish assessment surveys and identification of areas in which to focus at-sea observations for fishing mortality estimation, and provide the basis for first-ever designation of spiny dogfish essential fish habitat, despite US legal requirements for essential fish habitat designations since 1996. Identified areas of high bycatch may expedite spatial management by indicating areas in which directed spiny dogfish fisheries could be focused or, conversely, areas in which heightened conservation and catch accounting efforts would be most effective to prevent overfishing of this long-lived, late-maturing species.
C1 [Gasper, Jason R.; Kruse, Gordon H.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA.
RP Gasper, JR (reprint author), Natl Marine Fisheries Serv, Alaska Reg Off, POB 21668, Juneau, AK 99802 USA.
EM jason.gasper@noaa.gov
FU US Department of Agriculture New Crops Grant program [ALK-07-02]
FX Partial funding for this research was provided by US Department of
Agriculture New Crops Grant program (grant ALK-07-02). We thank the
North Pacific Observer Program, International Pacific Halibut
Commission, and the National Marine Fisheries Service for providing
fisheries and survey catch information used in the study, and two
anonymous reviewers, as well as Quentin Fong, Joshua Greenberg, and Marc
Miller, for reviews of the draft manuscript.
NR 42
TC 3
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U1 2
U2 27
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA
SN 0706-652X
EI 1205-7533
J9 CAN J FISH AQUAT SCI
JI Can. J. Fish. Aquat. Sci.
PD SEP
PY 2013
VL 70
IS 9
BP 1372
EP 1385
DI 10.1139/cjfas-2012-0535
PG 14
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 209LL
UT WOS:000323758200011
ER
PT J
AU Hulson, PJF
Quinn, TJ
Hanselman, DH
Ianelli, JN
AF Hulson, Peter-John F.
Quinn, Terrance J., II
Hanselman, Dana H.
Ianelli, James N.
TI Spatial modeling of Bering Sea walleye pollock with integrated
age-structured assessment models in a changing environment
SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES
LA English
DT Article
ID THERAGRA-CHALCOGRAMMA; STOCK ASSESSMENT; CLIMATE-CHANGE;
POPULATION-DYNAMICS; CATCH; MANAGEMENT; FISHERY; PATTERNS; WESTERN;
FUTURE
AB Climate change may affect the spatial distribution of fish populations in ways that would affect the accuracy of spatially aggregated age-structured assessment models. To evaluate such scenarios, spatially aggregated models were compared with spatially explicit models using simulations. These scenarios were based on hypothetical climate-driven distribution shifts and reductions in mean recruitment of walleye pollock (Gadus chalcogrammus) in the eastern Bering Sea. Results indicate that biomass estimates were reasonably accurate for both types of estimation models and precision improved with the inclusion of tagging data. Bias in some aggregated model scenarios could be attributed to unaccounted-for process errors in annual fishing mortality rates and was reduced when estimating effective sample size or time-varying selectivity. Spatially explicit models that allow estimation of variability in movement and ontogenetic parameters (specified as a random walk process) were shown to be feasible, whereas models that misspecified ontogenetic movement and climate change effects resulted in biased biomass and movement parameter estimates. These results illustrate that more complex models may characterize processes better but may be less robust for management advice.
C1 [Hulson, Peter-John F.; Quinn, Terrance J., II] Univ Alaska Fairbanks, Juneau Ctr, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA.
[Hulson, Peter-John F.; Hanselman, Dana H.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA.
[Ianelli, James N.] NOAA, Resource Ecol & Fisheries Management Div, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA.
RP Hulson, PJF (reprint author), NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM pete.hulson@noaa.gov
FU Alaska Sea Grant; National Oceanic and Atmospheric Administration Office
of Sea Grant, Department of Commerce [NA06OAR4170013, R/31-16,
NA10OAR4170097, R/31-19]; University of Alaska
FX This publication is the result of research sponsored by Alaska Sea Grant
with funds from the National Oceanic and Atmospheric Administration
Office of Sea Grant, Department of Commerce, under grant No.
NA06OAR4170013 (project No. R/31-16) and grant No. NA10OAR4170097
(project No. R/31-19), and from the University of Alaska with funds
appropriated by the State. We also thank Milo Adkison, Brenda Norcross,
Gary Marty, Jon Heifetz, and two anonymous reviewers for helpful
comments and advice. The findings and conclusions in this paper are
those of the authors and do not necessarily represent the views of the
National Marine Fisheries Service, NOAA.
NR 35
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U1 3
U2 15
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA
SN 0706-652X
J9 CAN J FISH AQUAT SCI
JI Can. J. Fish. Aquat. Sci.
PD SEP
PY 2013
VL 70
IS 9
BP 1402
EP 1416
DI 10.1139/cjfas-2013-0020
PG 15
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 209LL
UT WOS:000323758200014
ER
PT J
AU Haghighipour, N
Capen, S
Hinse, TC
AF Haghighipour, Nader
Capen, Stephanie
Hinse, Tobias C.
TI Detection of Earth-mass and super-Earth Trojan planets using transit
timing variation method
SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY
LA English
DT Article
DE Planetary systems; Stability analysis; MEGNO; Phase space structure;
Resonance; Periodic orbits; Numerical method; Kepler space telescope;
TTVs
ID SUN-LIKE STAR; TERRESTRIAL PLANETS; EXTRASOLAR PLANETS; 1/1 RESONANCE;
GLOBAL DYNAMICS; SYSTEMS; EXOPLANETS; EXOMOON; BODIES
AB We have carried out an extensive study of the possibility of the detection of Earth-mass and super-Earth Trojan planets using transit timing variation method with the Kepler space telescope. We have considered a system consisting of a transiting Jovian-type planet in a short period orbit, and determined the induced variations in its transit timing due to an Earth-mass/super-Earth Trojan planet. We mapped a large section of the phase space around the 1:1 mean-motion resonance and identified regions corresponding to several other mean-motion resonances where the orbit of the planet would be stable. We calculated transit timing variations (TTVs) for different values of the mass and orbital elements of the transiting and perturbing bodies as well as the mass of central star, and identified orbital configurations of these objects (ranges of their orbital elements and masses) for which the resulted TTVs would be within the range of the variations of the transit timing of Kepler's planetary candidates. Results of our study indicate that in general, the amplitudes of the TTVs fall within the detectable range of timing precision obtained from the Kepler's long-cadence data, and depending on the parameters of the system, their magnitudes may become as large as a few hours. The probability of detection is higher for super-Earth Trojans with slightly eccentric orbits around short-period Jovian-type planets with masses slightly smaller than Jupiter. We present the details of our study and discuss the implications of its results.
C1 [Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
[Capen, Stephanie] Univ Hawaii Manoa, Dept Educ, Honolulu, HI 96822 USA.
[Hinse, Tobias C.] Korea Astron & Space Sci Inst, Taejon 304358, South Korea.
[Hinse, Tobias C.] Armagh Observ, Armagh BT61 9DG, North Ireland.
RP Haghighipour, N (reprint author), Univ Hawaii Manoa, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM nader@ifa.hawaii.edu; stephaniecapen@gmail.com; tchinse@gmail.com
FU NASA EXOB Grant [NNX09AN05G]; NASA Astrobiology Institute at the
Institute for Astronomy (IfA), University of Hawaii [NNA09DA77A]; IfA
NSF; Korea Astronomy and Space Science Institute (KASI) [2012-1-410-02];
Korea Research Council for Fundamental Science and Technology (KRCF)
FX N.H. acknowledges support from NASA EXOB Grant NNX09AN05G and from the
NASA Astrobiology Institute under Cooperative Agreement NNA09DA77A at
the Institute for Astronomy (IfA), University of Hawaii. S. C.
acknowledges support from the IfA NSF-funded REU program. T. C. H.
acknowledges support from the Korea Astronomy and Space Science
Institute (KASI) Grant 2012-1-410-02 and the Korea Research Council for
Fundamental Science and Technology (KRCF) through the Young Research
Scientist Fellowship Program. The MEGNO computations were carried out at
the SFI/HEA Irish Center for High-End Computing (ICHEC) Center and the
PLUTO computing cluster at KASI. T. C. H. would also like to thank the
Institute for Astronomy and the NASA Astrobiology Institute at the
University of Hawaii-Manoa for their hospitality during the course of
this project.
NR 36
TC 6
Z9 6
U1 0
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0923-2958
J9 CELEST MECH DYN ASTR
JI Celest. Mech. Dyn. Astron.
PD SEP
PY 2013
VL 117
IS 1
SI SI
BP 75
EP 89
DI 10.1007/s10569-013-9510-y
PG 15
WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications
SC Astronomy & Astrophysics; Mathematics
GA 208CY
UT WOS:000323655200006
ER
PT J
AU Valencia, VA
Righter, K
Rosas-Elguera, J
Lopez-Martinez, M
Grove, M
AF Valencia, Victor A.
Righter, Kevin
Rosas-Elguera, Jose
Lopez-Martinez, Margarita
Grove, Marty
TI The age and composition of the pre-Cenozoic basement of the Jalisco
Block: implications for and relation to the Guerrero composite terrane
SO CONTRIBUTIONS TO MINERALOGY AND PETROLOGY
LA English
DT Article
DE Guerrero terrane; Jalisco Block; Granite; Quartzofeldspathic schist;
Mexican arc
ID MEXICAN VOLCANIC BELT; SOUTHWESTERN NORTH-AMERICA; PORPHYRY
COPPER-DEPOSIT; U-PB GEOCHRONOLOGY; LARGE OCEAN BASINS; BAJA-CALIFORNIA;
WESTERN MEXICO; ISOTOPE GEOCHEMISTRY; TECTONIC EVOLUTION; BASALTIC
VOLCANISM
AB The Jalisco Block is thought to be part of the Guerrero terrane, but the nature and age of the underlying crystalline basement are largely unknown. We have collected a suite of schists, granitoids, and weakly metamorphosed marine sediments from various parts of the Jalisco Block including Atenguillo and Ameca, Mascota and San Sebastian, Cuale, Puerto Vallarta, Punta Mita, Yelapa, and Tomatlan. The schists range in age from 135 to 161 Ma, with many exhibiting Proterozoic and Phanerozoic zircon ages. The granitoids range in age from 65 to 90 Ma, and are calc-alkaline compositionally-similar to granitoids from the Puerto Vallarta and Los Cabos batholiths. The Jalisco granitoids also experienced similar uplift rates to granitoids from the regions to the north and south of the Jalisco Block. The marine sediments yield a maximum depositional age of 131 Ma, and also contain a significant zircon population with ages extending back to the Archean. Granitoids from this study define two age groups, even after the effects of thermal resetting and different closure temperatures are considered. The 66.8-Ma silicic ash flow tuff near Union de Tula significantly expands the extent of this Cretaceous-Paleocene age ash flow tuff unit within the Jalisco Block, and we propose calling the unit "Carmichael silicic ash flow tuff volcanic succession" in honor of Ian Carmichael. The ages of the basement schists in the Jalisco Block fully overlap with the ages of terranes of continental Mexico, and other parts of the Guerrero terrane in the south, confirming the autochthonous origin of the Jalisco Block rather than exotic arc or allochthonous origin. Geologic data, in combination with geochronologic and oxygen isotopic data, suggest the evolution of SW Mexico with an early 200-1,200-Ma passive margin, followed by steep subduction in a continental arc setting at 160-165 Ma, then shallower subduction by 135 Ma, and finally, emplacement of granitoids at 65-90 Ma.
C1 [Valencia, Victor A.] Washington State Univ, Sch Environm, Pullman, WA 99164 USA.
[Righter, Kevin] NASA, Lyndon B Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA.
[Righter, Kevin] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Rosas-Elguera, Jose] Univ Guadalajara, Lab Interinst Magnetismo Nat, Guadalajara 44430, Jalisco, Mexico.
[Rosas-Elguera, Jose] Univ Guadalajara, Ctr Univ Valles, Ameca, Mexico.
[Lopez-Martinez, Margarita] CICESE, Dept Geol, Ensenada 22860, Baja California, Mexico.
[Grove, Marty] Stanford Univ, Stanford, CA 94305 USA.
RP Righter, K (reprint author), NASA, Lyndon B Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
RI UCLA, SIMS/A-1459-2011
FU University of Arizona Small Grants Program from office of the Vice
President for Research; CONACyT Ciencia Basica [CB-2009-01-00131191];
NSF International Programs [INT0420380]; Univ. of Arizona; LPI; USRA
FX I. S. E. Carmichael had a huge influence on KR and among other things
got him thinking about basement lithologies in Jalisco while undertaking
graduate studies at UC Berkeley in 1990-1994. Initial funding for this
project was provided by the University of Arizona Small Grants Program
from the office of the Vice President for Research. This initial help
was instrumental in getting this project supported in the way required
to carry out a comprehensive study. The study was supported by CONACyT
Ciencia Basica (CB-2009-01-00131191) and NSF International Programs
(INT0420380); for the latter, we thank H. Stolberg for his assistance,
as well as L. Lane (Univ. of Arizona), D. Cranford (LPI), and D. Devin
(USRA) for their assistance with financial issues. G. Gehrels and J.
Vervoort are thanked for being supportive of finalizing this study. M.
A. Garcia Garcia and A. S. Rosas Montoya helped with the Ar-Ar
experiments. Paul Wallace provided petrographic microscope images of
LV-250 that are in the online resource. The journal reviews of L.
Ferrari, F. Ortega-Gutierrez, and P. Schaaf were extremely helpful and
much appreciated. This is LPI Contribution No. 1734.
NR 98
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U1 0
U2 24
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0010-7999
J9 CONTRIB MINERAL PETR
JI Contrib. Mineral. Petrol.
PD SEP
PY 2013
VL 166
IS 3
BP 801
EP 824
DI 10.1007/s00410-013-0908-z
PG 24
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 206SB
UT WOS:000323541600008
ER
PT J
AU Verma, S
Payra, S
Gautam, R
Prakash, D
Soni, M
Holben, B
Bell, S
AF Verma, Sunita
Payra, Swagata
Gautam, Ritesh
Prakash, Divya
Soni, Manish
Holben, Brent
Bell, Shaun
TI Dust events and their influence on aerosol optical properties over
Jaipur in Northwestern India
SO ENVIRONMENTAL MONITORING AND ASSESSMENT
LA English
DT Article
DE Dust; Aerosols; Optical properties; Transport; Climate
ID 2009 PREMONSOON SEASON; PYRAMID 5079 M; CHEMICAL-COMPOSITION; ARABIAN
SEA; SIZE DISTRIBUTION; NORTHERN INDIA; GANGETIC BASIN; SOURCE AREAS;
DESERT DUST; M A.S.L.
AB In this study, we systematically document the link between dust episodes and local scale regional aerosol optical properties over Jaipur located in the vicinity of Thar Desert in the northwestern state of Rajasthan. The seasonal variation of AOT(500 nm) (aerosol optical thickness) shows high values (0.51 +/- 0.18) during pre-monsoon (dust dominant) season while low values (0.36 +/- 0.14) are exhibited during winter. The ngstrom wavelength exponent has been found to exhibit low value (< 0.25) indicating relative dominance of coarse-mode particles during pre-monsoon season. The AOT increased from 0.36 (April(mean)) to 0.575 (May-June(mean)). Consequently, volume concentration range increases from April through May-June followed by a sharp decline in July during the first active phase of the monsoon. Significantly high dust storms were observed over Jaipur as indicated by high values of single scattering albedo (SSA(440 nm) = 0.89, SSA(675 nm) = 0.95, SSA(870 nm) = 0.97, SSA(1,020 nm) = 0.976) than the previously reported values over IGP region sites. The larger SSA values (more scattering aerosol), especially at longer wavelengths, is due to the abundant dust loading, and is attributed to the measurement site's proximity to the Thar Desert. The mean and standard deviation in SSA and asymmetry parameter during pre-monsoon season over Jaipur is 0.938 +/- 0.023 and 0.712 +/- 0.017 at 675 nm wavelength, respectively. Back-trajectory air mass simulations suggest Thar Desert in northwestern India as the primary source of high aerosols dust loading over Jaipur region as well as contribution by long-range transport from the Arabian Peninsula and Middle East gulf regions, during pre-monsoon season.
C1 [Verma, Sunita; Payra, Swagata; Prakash, Divya] Birla Inst Technol Mesra, Ctr Excellence Climatol, Extens Ctr Jaipur, Jaipur 302017, Rajasthan, India.
[Gautam, Ritesh; Holben, Brent; Bell, Shaun] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Soni, Manish] Birla Inst Technol Mesra, Remote Sensing Div, Extens Ctr Jaipur, Jaipur 302017, Rajasthan, India.
[Bell, Shaun] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Verma, S (reprint author), Birla Inst Technol Mesra, Ctr Excellence Climatol, Extens Ctr Jaipur, Jaipur 302017, Rajasthan, India.
EM verma.sunita@gmail.com
FU Department of Science and Technology (DST), Govt. of India
[SR/S4/AS:39/2009]
FX We gratefully acknowledge and thank the AERONET group for making all the
data available in the form of Level 2.0 quality assured product after
necessary screening and post calibrations. The authors thank the NOAA
Air Resources Laboratory (ARL) for the provision of the HYSPLIT
transport and dispersion model and website
http://www.arl.noaa.gov/ready.php used in this publication. This
research was also supported by Department of Science and Technology
(DST), Govt. of India as a research grant under project
SR/S4/AS:39/2009. We also acknowledge wunderground.com and the India
Meteorological Department for providing the data. The first authors also
acknowledge the Vice Chancellor, BIT Prof Ajay Chakrabarty and Executive
Director Prof Purnendu Ghosh for providing the resources that enabled us
to carry out this study.
NR 52
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U1 0
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-6369
EI 1573-2959
J9 ENVIRON MONIT ASSESS
JI Environ. Monit. Assess.
PD SEP
PY 2013
VL 185
IS 9
BP 7327
EP 7342
DI 10.1007/s10661-013-3103-9
PG 16
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 192LI
UT WOS:000322485500018
PM 23397540
ER
PT J
AU Peterson, MJ
Mueter, F
Hanselman, D
Lunsford, C
Matkin, C
Fearnbach, H
AF Peterson, Megan J.
Mueter, Franz
Hanselman, Dana
Lunsford, Chris
Matkin, Craig
Fearnbach, Holly
TI Killer whale (Orcinus orca) depredation effects on catch rates of six
groundfish species: implications for commercial longline fisheries in
Alaska
SO ICES JOURNAL OF MARINE SCIENCE
LA English
DT Article
DE depredation; groundfish; killer whales; longline; marine mammals;
Pacific halibut; sablefish
ID TOOTHFISH DISSOSTICHUS-ELEGINOIDES; SOUTHEASTERN BERING-SEA; ADJACENT
WATERS; SOUTH GEORGIA; SPERM-WHALES; PHYSETER-MACROCEPHALUS; ALEUTIAN
ISLANDS; BRITISH-COLUMBIA; MARINE MAMMALS; FISHING GEAR
AB Killer whale (Orcinus orca) depredation occurs when whales damage or remove fish caught on longline gear. This study uses National Marine Fisheries Service longline survey data from 1998-2011 to explore spatial and temporal trends in killer whale depredation and to quantify the effect of killer whale depredation on catches of six groundfish species within three management areas in Alaska: the Bering Sea, Aleutian Islands and Western Gulf of Alaska. When killer whales were present during survey gear retrieval, whales removed an estimated 54-72% of sablefish (Anoplopoma fimbria), 41-84% of arrowtooth flounder (Atheresthes stomias) and 73% (Bering Sea only) of Greenland turbot (Reinhardtius hippoglossoides). Effects on Pacific halibut (Hippoglossus stenolepis) and Pacific cod (Gadus macrocephalus) were significant in the Western Gulf only with 51% and 46% reductions, respectively. Overall catches (depredated and non-depredated sets) for all groundfish species significantly impacted by killer whale depredation were lower by 9-28% (p, 0.05). Effects on shortspine thornyhead (Sebastolobus alascanus) catches were not significant in any management area (p. 0.05). These results provide insight into the potential impacts of killer whale depredation on fish stock abundance indices and commercially important fisheries in Alaska and will inform future research on apex predator-fisheries interactions.
C1 [Peterson, Megan J.; Mueter, Franz] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA.
[Hanselman, Dana; Lunsford, Chris] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA.
[Matkin, Craig] North Gulf Ocean Soc, Homer, AK 99603 USA.
[Fearnbach, Holly] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Natl Marine Mammal Lab, Seattle, WA 98115 USA.
RP Peterson, MJ (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, 17101 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM mjpeterson6@alaska.edu
FU National Marine Fisheries Service; Rasmuson Fisheries Research Center;
National Science Foundation (NSF) Marine Ecosystem Sustainability in the
Arctic and Subarctic (MESAS) IGERT [DGE-0801720]; NSF Arctic Social
Sciences Program [1107401]
FX This research received funding from the National Marine Fisheries
Service, and was also supported by the Rasmuson Fisheries Research
Center, the National Science Foundation (NSF) Marine Ecosystem
Sustainability in the Arctic and Subarctic (MESAS) IGERT (Award
DGE-0801720), and the NSF Arctic Social Sciences Program (Award
1107401).
NR 56
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U1 2
U2 46
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 1054-3139
EI 1095-9289
J9 ICES J MAR SCI
JI ICES J. Mar. Sci.
PD SEP
PY 2013
VL 70
IS 6
BP 1220
EP 1232
DI 10.1093/icesjms/fst045
PG 13
WC Fisheries; Marine & Freshwater Biology; Oceanography
SC Fisheries; Marine & Freshwater Biology; Oceanography
GA 207WO
UT WOS:000323635600018
ER
PT J
AU Pinchuk, AI
Coyle, KO
Farley, EV
Renner, HM
AF Pinchuk, Alexei I.
Coyle, Kenneth O.
Farley, Edward V.
Renner, Heather M.
TI Emergence of the Arctic Themisto libellula (Amphipoda: Hyperiidae) on
the southeastern Bering Sea shelf as a result of the recent cooling, and
its potential impact on the pelagic food web
SO ICES JOURNAL OF MARINE SCIENCE
LA English
DT Article
DE Themisto libellula; Bering Sea; climate change
ID OSCILLATING CONTROL HYPOTHESIS; MARGINAL ICE-ZONE; BARENTS SEA;
ST-LAWRENCE; NORTH PACIFIC; ZOOPLANKTON; ECOSYSTEM; VARIABILITY; GROWTH;
ALASKA
AB The eastern Bering Sea shelf experienced a sequence of warm years after a regime shift in the late 1970s. Following a series of unusually warm years in the early 2000s, the climate shifted again in 2007 to a series of extremely cold years that were marked by intense ice coverage and late ice retreat. Spatial and temporal variability in zooplankton communities during the recent cold period was investigated as part of the collaborative BEST-BSIERP program. An increasing presence of the Arctic hyperiid Themisto libellula, which had not been reported from the southeastern Bering Sea since the 1970s, was observed in the Middle Shelf Domain, indicating a developing structural shift in the zooplankton community in response to continuous cold conditions. Simultaneously, T. libellula became an increasingly dominant prey in the diets of zooplanktivorous fish and seabirds, demonstrating the important role for T. libellula in the pelagic food web. Our analysis suggests that T. libellula is capable of controlling copepod populations, thus it may become a potential contributor to top-down regulation of Calanus spp. in the eastern Bering Sea.
C1 [Pinchuk, Alexei I.] Univ Alaska, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA.
[Coyle, Kenneth O.] Univ Alaska, Sch Fisheries & Ocean Sci, Fairbanks, AK 99775 USA.
[Farley, Edward V.] Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Lab, Juneau, AK 99801 USA.
[Renner, Heather M.] Alaska Maritime NWR, Homer, AK 99603 USA.
RP Pinchuk, AI (reprint author), Univ Alaska, Sch Fisheries & Ocean Sci, 17101 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM aipinchuk@alaska.edu
FU National Science Foundation as part of the BEST program [ARC-0816805,
ARC-0946402, ARC-1107203]; North Pacific Research Board;
Arctic-Yukon-Kuskokwim Sustainable Salmon Initiative [AYICSI-NA16FP2993]
FX Zooplankton collections were supported by the National Science
Foundation as part of the BEST program (Award Nos. ARC-0816805,
ARC-0946402 and ARC-1107203). BASIS efforts were conducted by the
National Marine Fisheries Service and funded by the North Pacific
Research Board and the Arctic-Yukon-Kuskokwim Sustainable Salmon
Initiative (Award No. AYICSI-NA16FP2993).
NR 66
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U2 22
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 1054-3139
EI 1095-9289
J9 ICES J MAR SCI
JI ICES J. Mar. Sci.
PD SEP
PY 2013
VL 70
IS 6
BP 1244
EP 1254
DI 10.1093/icesjms/fst031
PG 11
WC Fisheries; Marine & Freshwater Biology; Oceanography
SC Fisheries; Marine & Freshwater Biology; Oceanography
GA 207WO
UT WOS:000323635600020
ER
PT J
AU Fox, S
Foisy, I
Venegas, RD
Pastoriza, BEG
Graham, RT
Hoffmayer, ER
Holmberg, J
Pierce, SJ
AF Fox, S.
Foisy, I.
De La Parra Venegas, R.
Galvan Pastoriza, B. E.
Graham, R. T.
Hoffmayer, E. R.
Holmberg, J.
Pierce, S. J.
TI Population structure and residency of whale sharks Rhincodon typus at
Utila, Bay Islands, Honduras
SO JOURNAL OF FISH BIOLOGY
LA English
DT Article
DE Atlantic; movement; philopatry; sexual segregation; site fidelity
ID GULF-OF-MEXICO; DIVING BEHAVIOR; INDIAN-OCEAN; IDENTIFICATION;
CONSERVATION; PATTERNS; REEF; SIZE; PHOTOIDENTIFICATION; AGGREGATION
AB There were 479 reported whale shark Rhincodon typus encounters between 1999 and 2011 at the island of Utila, which forms part of the Meso-American Barrier Reef System (MBRS) in the western Caribbean Sea. The majority of R. typus were found to feed on small bait fish associated with various tuna species. Ninety-five individual R. typus, ranging from 2 to 11 m total length (L-T), were identified through their unique spot patterns. A significant male bias (65%) was present. There was no significant difference between the mean +/- S.D. L-T of female (6.66 +/- 1.65 m) and male (6.25 +/- 1.60 m) R. typus. Most R. typus were transient to Utila, with 78% sighted only within a single calendar year, although some individuals were sighted in up to 5 years. Mean residency time was modelled to be 11.76 days using maximum likelihood methods. (C) 2013 The Fisheries Society of the British Isles
C1 [Fox, S.; Foisy, I.] Utila Whale Shark Res, Utila, Honduras.
[De La Parra Venegas, R.; Galvan Pastoriza, B. E.] Ch Ooj Ajauil AC, Cancun, Quintana Roo, Mexico.
[Graham, R. T.] Wildlife Conservat Soc, Gulf & Caribbean Sharks & Rays Program, Punta Gorda, Belize.
[Hoffmayer, E. R.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA.
[Holmberg, J.; Pierce, S. J.] ECOCEAN USA, Portland, OR 97217 USA.
[Pierce, S. J.] Marine Megafauna Fdn, Tofo Beach, Inhambane, Mozambique.
RP Pierce, SJ (reprint author), ECOCEAN USA, 1726 N Terry St, Portland, OR 97217 USA.
EM simon@marinemegafauna.org
FU Office of Naval Research [N0270A]; Deep Blue Resort; Swiss Shark
Foundation
FX Thanks to all of the organizations and individuals that submitted
sighting data to the ECOCEAN Global Whale Shark Photo-Identification
Database, particularly the Whale Shark and Oceanic Research Center in
Utila. S.J.P.'s work on this study was supported by Deep Blue Resort,
the Swiss Shark Foundation and private donors. Funding for the further
development of one of the software tools used in this study (the
Shepherd Project) was provided by the Office of Naval Research (contract
N0270A to C. S. Baker and D. Wright) as a part of the geneGIS Project.
We are grateful to the two anonymous reviewers for their constructive
comments which have improved this work.
NR 52
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U1 5
U2 59
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-1112
J9 J FISH BIOL
JI J. Fish Biol.
PD SEP
PY 2013
VL 83
IS 3
BP 574
EP 587
DI 10.1111/jfb.12195
PG 14
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 209CP
UT WOS:000323732100010
PM 23991875
ER
PT J
AU Huang, HS
Walker, ND
Hsueh, Y
Chao, Y
Leben, RR
AF Huang, Haosheng
Walker, Nan D.
Hsueh, Ya
Chao, Yi
Leben, Robert R.
TI An Analysis of Loop Current Frontal Eddies in a ?degrees Atlantic Ocean
Model Simulation
SO JOURNAL OF PHYSICAL OCEANOGRAPHY
LA English
DT Article
DE Eddies; Empirical orthogonal functions; Time series; General circulation
models
ID GULF-OF-MEXICO; YUCATAN CHANNEL; POTENTIAL VORTICITY; CYCLONIC EDDIES;
CARIBBEAN SEA; STREAM SYSTEM; FLOW; VARIABILITY; CIRCULATION; VORTEX
AB The Loop Current frontal eddies (LCFEs) refer to cyclonic cold eddies moving downstream along the outside edge of the Loop Current in the eastern Gulf of Mexico. They have been observed by in situ measurements and satellite imagery, mostly downstream of the Campeche Bank continental shelf. Their evolution, simulated by a primitive equation ?degrees and 37-level Atlantic Ocean general circulation numerical model, is described in detail in this study. Some of the simulated LCFEs arise, with the passage through the Yucatan Channel of a Caribbean anticyclonic eddy, as weak cyclones with diameters less than 100 km near the Yucatan Channel. They then grow to fully developed eddies with diameters on the order of 150-200 km while moving along the Loop Current edge. Modeled LCFEs have a very coherent vertical structure with isotherm doming seen from 50- to similar to 1000-m depth. The Caribbean anticyclone and LCFE are two predominant features in this numerical model simulation, which account for 22% and 10%, respectively, of the short-term (period less than 100 days) temperature variance at 104.5 m in the complex empirical orthogonal function (CEOF) analysis. The source water inside the LCFEs that are generated by Caribbean anticyclonic eddy impingement can be traced back, using a backward-in-time Lagrangian particle-tracking method, to the western edge of the Caribbean Current in the northwest Caribbean Sea and to coastal waters near the northern Yucatan Peninsula. The model results indicating a pairing of anticyclonic and cyclonic eddies within and north of the Yucatan Channel are supported by satellite altimetry measurements during February 2002 when several altimeters were operational.
C1 [Huang, Haosheng; Walker, Nan D.] Louisiana State Univ, Sch Coast & Environm, Dept Oceanog & Coastal Sci, Baton Rouge, LA 70803 USA.
[Hsueh, Ya] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Chao, Yi] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Leben, Robert R.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA.
RP Huang, HS (reprint author), Louisiana State Univ, Sch Coast & Environm, Dept Oceanog & Coastal Sci, 320 Howe Russell Geosci Complex, Baton Rouge, LA 70803 USA.
EM hhuang7@lsu.edu
FU Minerals Management Service [14-35-0001-30804]; Office of Naval Research
[N00014-00-1-0406]; National Aeronautics and Space Administration (NASA)
FX The research was supported by the Minerals Management Service
Cooperative Agreement 14-35-0001-30804 and by the Office of Naval
Research Grant N00014-00-1-0406. The numerical modeling research
described in this publication was carried out, in part, at the Jet
Propulsion Laboratory (JPL), California Institute of Technology, under a
contract with the National Aeronautics and Space Administration (NASA).
Computations were performed on the supercomputer provided through the
JPL Supercomputing Project. We thank Chet Pilley at Earth Scan
Laboratory, Louisiana State University, for processing the altimetry sea
surface height images.
NR 61
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U1 1
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-3670
EI 1520-0485
J9 J PHYS OCEANOGR
JI J. Phys. Oceanogr.
PD SEP
PY 2013
VL 43
IS 9
BP 1924
EP 1939
DI 10.1175/JPO-D-12-0227.1
PG 16
WC Oceanography
SC Oceanography
GA 211FU
UT WOS:000323891800006
ER
PT J
AU Korkin, SV
Lyapustin, AI
Rozanov, VV
AF Korkin, Sergey V.
Lyapustin, Alexei I.
Rozanov, Vladimir V.
TI APC: A new code for Atmospheric Polarization Computations
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Polarization; Modification of the discrete ordinates method; Surface
reflection
ID RADIATIVE-TRANSFER CODE; SPHERICAL-HARMONICS SOLUTION; SCATTERING
ATMOSPHERE; MULTIPLE-SCATTERING; TRANSFER EQUATION; RAYLEIGH-SCATTERING;
SOLAR-RADIATION; TRANSFER MODELS; LIGHT; RETRIEVAL
AB A new polarized radiative transfer code Atmospheric Polarization Computations (APC) is described. The code is based on separation of the diffuse light field into anisotropic and smooth (regular) parts. The anisotropic part is computed analytically. The smooth regular part is computed numerically using the discrete ordinates method. Vertical stratification of the atmosphere, common types of bidirectional surface reflection and scattering by spherical particles or spheroids are included. A particular consideration is given to computation of the bidirectional polarization distribution function (BPDF) of the waved ocean surface. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Korkin, Sergey V.] Univ Space Res Assoc, GESTAR, Columbia, MD USA.
[Korkin, Sergey V.; Lyapustin, Alexei I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Rozanov, Vladimir V.] Univ Bremen, Inst Remote Sensing, D-28359 Bremen, Germany.
RP Korkin, SV (reprint author), NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD USA.
EM sergey.v.korkin@nasa.gov
RI Lyapustin, Alexei/H-9924-2014
OI Lyapustin, Alexei/0000-0003-1105-5739
NR 61
TC 3
Z9 3
U1 0
U2 11
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 SEP
PY 2013
VL 127
BP 1
EP 11
DI 10.1016/j.jqsrt.2013.06.019
PG 11
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 207GD
UT WOS:000323586000001
ER
PT J
AU Yi, BQ
Yang, P
Baum, BA
L'Ecuyer, T
Oreopoulos, L
Mlawer, EJ
Heymsfield, AJ
Liou, KN
AF Yi, Bingqi
Yang, Ping
Baum, Bryan A.
L'Ecuyer, Tristan
Oreopoulos, Lazaros
Mlawer, Eli J.
Heymsfield, Andrew J.
Liou, Kuo-Nan
TI Influence of Ice Particle Surface Roughening on the Global Cloud
Radiative Effect
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Cloud forcing; Ice crystals; Optical properties; Radiative forcing
ID SINGLE-SCATTERING PROPERTIES; GENERAL-CIRCULATION MODEL; CIRRUS CLOUDS;
CLIMATE MODELS; OPTICAL-PROPERTIES; LIGHT-SCATTERING; ACCURATE
PARAMETERIZATION; NATURAL CLOUDS; CRYSTALS; RETRIEVAL
AB Ice clouds influence the climate system by changing the radiation budget and large-scale circulation. Therefore, climate models need to have an accurate representation of ice clouds and their radiative effects. In this paper, new broadband parameterizations for ice cloud bulk scattering properties are developed for severely roughened ice particles. The parameterizations are based on a general habit mixture that includes nine habits (droxtals, hollow/solid columns, plates, solid/hollow bullet rosettes, aggregate of solid columns, and small/large aggregates of plates). The scattering properties for these individual habits incorporate recent advances in light-scattering computations. The influence of ice particle surface roughness on the ice cloud radiative effect is determined through simulations with the Fu-Liou and the GCM version of the Rapid Radiative Transfer Model (RRTMG) codes and the National Center for Atmospheric Research Community Atmosphere Model (CAM, version 5.1). The differences in shortwave (SW) and longwave (LW) radiative effect at both the top of the atmosphere and the surface are determined for smooth and severely roughened ice particles. While the influence of particle roughening on the single-scattering properties is negligible in the LW, the results indicate that ice crystal roughness can change the SW forcing locally by more than 10 W m(-2) over a range of effective diameters. The global-averaged SW cloud radiative effect due to ice particle surface roughness is estimated to be roughly 1-2 W m(-2). The CAM results indicate that ice particle roughening can result in a large regional SW radiative effect and a small but nonnegligible increase in the global LW cloud radiative effect.
C1 [Yi, Bingqi; Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Baum, Bryan A.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
[L'Ecuyer, Tristan] Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI USA.
[Oreopoulos, Lazaros] NASA, Climate & Radiat Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Mlawer, Eli J.] Atmospher & Environm Res Inc, Lexington, MA USA.
[Heymsfield, Andrew J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Liou, Kuo-Nan] Univ Calif Los Angeles, Joint Inst Earth Syst Sci & Engn, Los Angeles, CA USA.
[Liou, Kuo-Nan] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
RP Yang, P (reprint author), Texas A&M Univ, Dept Atmospher Sci, TAMU 3150, College Stn, TX 77843 USA.
EM pyang@tamu.edu
RI Yang, Ping/B-4590-2011; Baum, Bryan/B-7670-2011; Heymsfield,
Andrew/E-7340-2011; Oreopoulos, Lazaros/E-5868-2012; Yi,
Bingqi/E-4076-2012; L'Ecuyer, Tristan/E-5607-2012
OI Baum, Bryan/0000-0002-7193-2767; Oreopoulos,
Lazaros/0000-0001-6061-6905; Yi, Bingqi/0000-0002-1437-8376; L'Ecuyer,
Tristan/0000-0002-7584-4836
FU NASA [NNX11AF40G, NNX11AK37G]; NASA's Modeling Analysis and Prediction
Program
FX The authors are grateful for Dr. Andrew Gettelman for his valuable
comments and suggestions. The Texas A&M Supercomputing Facility
(http://sc.tamu.edu/) provided computing resources for performing the
model simulation reported in this paper. Bryan Baum and Ping Yang
acknowledge support from NASA Grant NNX11AF40G. Ping Yang also
acknowledges support from NASA Grant NNX11AK37G. Lazaros Oreopoulos is
supported by NASA's Modeling Analysis and Prediction Program.
NR 50
TC 27
Z9 27
U1 2
U2 17
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD SEP
PY 2013
VL 70
IS 9
BP 2794
EP 2807
DI 10.1175/JAS-D-13-020.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 211FJ
UT WOS:000323890400008
ER
PT J
AU Mielke, RE
Priester, JH
Werlin, RA
Gelb, J
Horst, AM
Orias, E
Holden, PA
AF Mielke, Randall E.
Priester, John H.
Werlin, Rebecca A.
Gelb, Jeff
Horst, Allison M.
Orias, Eduardo
Holden, Patricia A.
TI Differential Growth of and Nanoscale TiO2 Accumulation in Tetrahymena
thermophila by Direct Feeding versus Trophic Transfer from Pseudomonas
aeruginosa
SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY
LA English
DT Article
ID OXIDE NANOPARTICLES; ESCHERICHIA-COLI; TITANIUM-DIOXIDE; QUANTUM DOTS;
ENGINEERED NANOMATERIALS; FOOD-WEB; BACTERIA; PROTOZOA; WATER; MODEL
AB Nanoscale titanium dioxide (TiO2) is increasingly used in consumer goods and is entering waste streams, thereby exposing and potentially affecting environmental microbes. Protozoans could either take up TiO2 directly from water and sediments or acquire TiO2 during bactivory (ingestion of bacteria) of TiO2-encrusted bacteria. Here, the route of exposure of the ciliated protozoan Tetrahymena thermophila to TiO2 was varied and the growth of, and uptake and accumulation of TiO2 by, T. thermophila were measured. While TiO2 did not affect T. thermophila swimming or cellular morphology, direct TiO2 exposure in rich growth medium resulted in a lower population yield. When TiO2 exposure was by bactivory of Pseudomonas aeruginosa, the T. thermophila population yield and growth rate were lower than those that occurred during the bactivory of non-TiO2-encrusted bacteria. Regardless of the feeding mode, T. thermophila cells internalized TiO2 into their food vacuoles. Biomagnification of TiO2 was not observed; this was attributed to the observation that TiO2 appeared to be unable to cross the food vacuole membrane and enter the cytoplasm. Nevertheless, our findings imply that TiO2 could be transferred into higher trophic levels within food webs and that the food web could be affected by the decreased growth rate and yield of organisms near the base of the web.
C1 [Mielke, Randall E.; Priester, John H.; Horst, Allison M.; Holden, Patricia A.] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Earth Res Inst, Santa Barbara, CA 93106 USA.
[Mielke, Randall E.; Priester, John H.; Horst, Allison M.; Holden, Patricia A.] Univ Calif Santa Barbara, UC Ctr Environm Implicat Nanotechnol UC CEIN, Santa Barbara, CA 93106 USA.
[Mielke, Randall E.] NASA, CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Werlin, Rebecca A.; Orias, Eduardo] Univ Calif Santa Barbara, Dept Mol Cellular & Dev Biol, Santa Barbara, CA 93106 USA.
[Gelb, Jeff] Xradia Corp, Pleasanton, CA USA.
RP Holden, PA (reprint author), Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Earth Res Inst, Santa Barbara, CA 93106 USA.
EM holden@bren.ucsb.edu
FU National Science Foundation [BES-9977772, DBI-0216480, MCB-1025069];
Environmental Protection Agency [0830117]
FX This research was funded primarily by the National Science Foundation
and the Environmental Protection Agency under cooperative agreement
DBI-0830117. Any opinions, findings, and conclusions or recommendations
expressed in this material are ours and do not necessarily reflect the
views of either the National Science Foundation or the Environmental
Protection Agency. This work has not been subjected to Environmental
Protection Agency review, and no official endorsement should be
inferred.; ESEM and STEM were partly performed in the
Micro-Environmental Imaging and Analysis Facility at the University of
California Santa Barbara (www.bren.ucsb.edu/facilities/MEIAF/) under
National Science Foundation awards BES-9977772 and DBI-0216480. Funding
to E.O. was provided by National Science Foundation award MCB-1025069.
NR 51
TC 19
Z9 19
U1 4
U2 59
PU AMER SOC MICROBIOLOGY
PI WASHINGTON
PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA
SN 0099-2240
J9 APPL ENVIRON MICROB
JI Appl. Environ. Microbiol.
PD SEP
PY 2013
VL 79
IS 18
BP 5616
EP 5624
DI 10.1128/AEM.01680-13
PG 9
WC Biotechnology & Applied Microbiology; Microbiology
SC Biotechnology & Applied Microbiology; Microbiology
GA 205DO
UT WOS:000323421900023
PM 23851096
ER
PT J
AU Masek, JG
Goward, SN
Kennedy, RE
Cohen, WB
Moisen, GG
Schleeweis, K
Huang, CQ
AF Masek, Jeffrey G.
Goward, Samuel N.
Kennedy, Robert E.
Cohen, Warren B.
Moisen, Gretchen G.
Schleeweis, Karen
Huang, Chengquan
TI United States Forest Disturbance Trends Observed Using Landsat Time
Series
SO ECOSYSTEMS
LA English
DT Article
DE forest disturbance; remote sensing; landsat; forest ecology
ID TROPICAL DEFORESTATION; CLIMATE-CHANGE; SATELLITE DATA; NORTH-AMERICA;
COVER LOSS; IMAGERY; BIODIVERSITY; SIMULATION; STRATEGIES; INVENTORY
AB Disturbance events strongly affect the composition, structure, and function of forest ecosystems; however, existing US land management inventories were not designed to monitor disturbance. To begin addressing this gap, the North American Forest Dynamics (NAFD) project has examined a geographic sample of 50 Landsat satellite image time series to assess trends in forest disturbance across the conterminous United States for 1985-2005. The geographic sample design used a probability-based scheme to encompass major forest types and maximize geographic dispersion. For each sample location disturbance was identified in the Landsat series using the Vegetation Change Tracker (VCT) algorithm. The NAFD analysis indicates that, on average, 2.77 Mha y(-1) of forests were disturbed annually, representing 1.09% y(-1) of US forestland. These satellite-based national disturbance rates estimates tend to be lower than those derived from land management inventories, reflecting both methodological and definitional differences. In particular, the VCT approach used with a biennial time step has limited sensitivity to low-intensity disturbances. Unlike prior satellite studies, our biennial forest disturbance rates vary by nearly a factor of two between high and low years. High western US disturbance rates were associated with active fire years and insect activity, whereas variability in the east is more strongly related to harvest rates in managed forests. We note that generating a geographic sample based on representing forest type and variability may be problematic because the spatial pattern of disturbance does not necessarily correlate with forest type. We also find that the prevalence of diffuse, non-stand-clearing disturbance in US forests makes the application of a biennial geographic sample problematic. Future satellite-based studies of disturbance at regional and national scales should focus on wall-to-wall analyses with annual time step for improved accuracy.
C1 [Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab Code 618, Greenbelt, MD 20771 USA.
[Goward, Samuel N.; Schleeweis, Karen; Huang, Chengquan] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Kennedy, Robert E.] Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA.
[Cohen, Warren B.] USDA Forest Serv, Pacific NW Res Stn, Corvallis, OR 97331 USA.
[Moisen, Gretchen G.] USDA Forest Serv, Rocky Mt Res Stn, Ogden, UT 84403 USA.
RP Masek, JG (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab Code 618, Greenbelt, MD 20771 USA.
EM Jeffrey.G.Masek@nasa.gov
RI Masek, Jeffrey/D-7673-2012;
OI Huang, Chengquan/0000-0003-0055-9798
FU NASA Terrestrial Ecology Program; NASA Applied Sciences Program; US
Forest Service (NASA) [NNG05GE55, NNX08AI26G, NNH11AR291]
FX This study was supported by the NASA Terrestrial Ecology and Applied
Sciences Programs and the US Forest Service (NASA Grants NNG05GE55 and
NNX08AI26G for Goward, Huang, and Schleeweis; Interagency Agreement
NNH11AR291 for Cohen). John Dwyer (USGS) is thanked for facilitating
data access and addressing questions related to Landsat data quality.
Eric Vermote (University of Maryland) and Greg Ederer (NASA GSFC)
provided support for the Landsat preprocessing and atmospheric
correction.
NR 57
TC 40
Z9 41
U1 9
U2 97
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1432-9840
J9 ECOSYSTEMS
JI Ecosystems
PD SEP
PY 2013
VL 16
IS 6
BP 1087
EP 1104
DI 10.1007/s10021-013-9669-9
PG 18
WC Ecology
SC Environmental Sciences & Ecology
GA 202UU
UT WOS:000323246000012
ER
PT J
AU Sridharan, D
Chappell, L
Wilson, W
Whalen, M
Cucinotta, F
Pluth, J
AF Sridharan, D.
Chappell, L.
Wilson, W.
Whalen, M.
Cucinotta, F.
Pluth, J.
TI Genomic Instability Elicited by the Mutagenic Heavy Ions in Space
Differs with Cell Type and Radiation Quality.
SO ENVIRONMENTAL AND MOLECULAR MUTAGENESIS
LA English
DT Meeting Abstract
CT 44th Annual Meeting of the
Environmental-Mutagenesis-and-Genomics-Society (EMGS)
CY SEP 21-25, 2013
CL Monterey, CA
SP Environm Mutagenesis & Genom Soc (EMGS)
C1 [Sridharan, D.; Wilson, W.; Whalen, M.; Pluth, J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Chappell, L.; Cucinotta, F.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0893-6692
J9 ENVIRON MOL MUTAGEN
JI Environ. Mol. Mutagen.
PD SEP
PY 2013
VL 54
SU 1
BP S55
EP S55
PG 1
WC Environmental Sciences; Genetics & Heredity; Toxicology
SC Environmental Sciences & Ecology; Genetics & Heredity; Toxicology
GA 205FV
UT WOS:000323429400172
ER
PT J
AU Choi, KK
Jhabvala, MD
Forrai, DP
Waczynski, A
Sun, J
Jones, R
AF Choi, Kwong-Kit
Jhabvala, Murzy D.
Forrai, David P.
Waczynski, Augustyn
Sun, Jason
Jones, Robert
TI Electromagnetic Modeling and Design of Quantum Well Infrared
Photodetectors
SO IEEE JOURNAL OF SELECTED TOPICS IN QUANTUM ELECTRONICS
LA English
DT Article
DE Electromagnetic field modeling; infrared detector; quantum efficiency
(QE)
AB The quantum efficiency (QE) of a quantum well infrared photodetector (QWIP) is historically difficult to predict and optimize. This difficulty is due to the lack of a quantitative model to calculate QE for a given detector structure. In this paper, we found that by expressing QE in terms of a volumetric integral of the vertical electric field, the QE can be readily evaluated using a finite element electromagnetic solver. We applied this model to all known QWIP structures in the literature and found good agreement with experiment in all cases. Furthermore, the model agrees with other theoretical solutions, such as the classical solution and the modal transmission-line solution when they are available. Therefore, we have established the validity of this model, and it can now be used to design new detector structures with the potential to greatly improve the detector QE.
C1 [Choi, Kwong-Kit; Sun, Jason] US Army Res Lab, Adelphi, MD 20833 USA.
[Jhabvala, Murzy D.; Waczynski, Augustyn] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Forrai, David P.; Jones, Robert] L 3 Cincinnati Elect, Mason, OH 45040 USA.
RP Choi, KK (reprint author), US Army Res Lab, Adelphi, MD 20833 USA.
EM kwong.k.choi.civ@mail.mil; Murzy.D.Jhabvala@nasa.gov;
Dave.Forrai@L-3Com.com; augustyn.waczynski-1@nasa.gov;
guifu.n.sun.civ@mail.mil; Robert.Jones@L-3Com.com
RI Choi, Kwong-Kit/K-9205-2013
NR 19
TC 3
Z9 5
U1 0
U2 25
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1077-260X
J9 IEEE J SEL TOP QUANT
JI IEEE J. Sel. Top. Quantum Electron.
PD SEP-OCT
PY 2013
VL 19
IS 5
DI 10.1109/JSTQE.2012.2216861
PG 10
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 202JM
UT WOS:000323210900029
ER
PT J
AU Ryoo, JM
Kaspi, Y
Waugh, DW
Kiladis, GN
Waliser, DE
Fetzer, EJ
Kim, J
AF Ryoo, Ju-Mee
Kaspi, Yohai
Waugh, Darryn W.
Kiladis, George N.
Waliser, Duane E.
Fetzer, Eric J.
Kim, Jinwon
TI Impact of Rossby Wave Breaking on U.S. West Coast Winter Precipitation
during ENSO Events
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Dry intrusions; ENSO; Rossby waves; Precipitation
ID POTENTIAL VORTICITY INTRUSIONS; UPPER-TROPOSPHERIC HUMIDITY;
SOUTHWESTERN UNITED-STATES; NINO-SOUTHERN-OSCILLATION; EASTERN TROPICAL
PACIFIC; EL-NINO; ATMOSPHERIC RIVERS; NORTH PACIFIC; CLIMATE-CHANGE;
ENERGY BUDGET
AB This study demonstrates that water vapor transport and precipitation are largely modulated by the intensity of the subtropical jet, transient eddies, and the location of wave breaking events during the different phases of ENSO. Clear differences are found in the potential vorticity (PV), meteorological fields, and trajectory pathways between the two different phases. Rossby wave breaking events have cyclonic and anticyclonic regimes, with associated differences in the frequency of occurrence and the dynamic response. During La Nina, there is a relatively weak subtropical jet allowing PV to intrude into lower latitudes over the western United States. This induces a large amount of moisture transport inland ahead of the PV intrusions, as well as northward transport to the west of a surface anticyclone. During El Nino, the subtropical jet is relatively strong and is associated with an enhanced cyclonic wave breaking. This is accompanied by a time-mean surface cyclone, which brings zonal moisture transport to the western United States. In both (El Nino and La Nina) phases, there is a high correlation (>0.3-0.7) between upper-level PV at 250 hPa and precipitation over the west coast of the United States with a time lag of 0-1 days. Vertically integrated water vapor fluxes during El Nino are up to 70 kg m(-1) s(-1) larger than those during La Nina along the west coast of the United States. The zonal and meridional moist static energy flux resembles wave vapor transport patterns, suggesting that they are closely controlled by the large-scale flows and location of wave breaking events during the different phase of ENSO.
C1 [Ryoo, Ju-Mee] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Kaspi, Yohai] Weizmann Inst Sci, Dept Environm Sci & Energy Res, IL-76100 Rehovot, Israel.
[Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Kiladis, George N.] NOAA, Div Phys Sci, Earth Syst Res Lab, Boulder, CO USA.
[Waliser, Duane E.; Fetzer, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Waliser, Duane E.; Kim, Jinwon] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
RP Ryoo, JM (reprint author), Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
EM jryoo@berkeley.edu
RI Waugh, Darryn/K-3688-2016
OI Waugh, Darryn/0000-0001-7692-2798
FU National Aeronautics and Space Administration (NASA)
FX We give special thanks to Tapio Schneider for helping to improve the
paper with insightful comments. We thank Bjorn Lambrigtsen for his
support and supervision. We also thank Inez Fung for helpful discussions
and the anonymous reviewers for helpful comments. The research
contributions from J.-M. Ryoo, D. E. Waliser, and E. J. Fetzer for this
study were performed at Jet Propulsion Laboratory (JPL), California
Institute of Technology (Caltech), under a contract with the National
Aeronautics and Space Administration (NASA).
NR 71
TC 14
Z9 14
U1 1
U2 22
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 SEP
PY 2013
VL 26
IS 17
BP 6360
EP 6382
DI 10.1175/JCLI-D-12-00297.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 205AK
UT WOS:000323412300010
ER
PT J
AU Geller, MA
Alexander, MJ
Love, PT
Bacmeister, J
Ern, M
Hertzog, A
Manzini, E
Preusse, P
Sato, K
Scaife, AA
Zhou, TH
AF Geller, Marvin A.
Alexander, M. Joan
Love, Peter T.
Bacmeister, Julio
Ern, Manfred
Hertzog, Albert
Manzini, Elisa
Preusse, Peter
Sato, Kaoru
Scaife, Adam A.
Zhou, Tiehan
TI A Comparison between Gravity Wave Momentum Fluxes in Observations and
Climate Models
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Gravity waves; Climate models
ID OFFICE UNIFIED MODEL; STRATOSPHERIC BALLOON FLIGHTS; GENERAL-CIRCULATION
MODEL; MIDDLE ATMOSPHERE; SPECTRAL PARAMETERIZATION; GLOBAL CLIMATE;
MAECHAM5 MODEL; PHASE SPEEDS; PART I; DRAG
AB For the first time, a formal comparison is made between gravity wave momentum fluxes in models and those derived from observations. Although gravity waves occur over a wide range of spatial and temporal scales, the focus of this paper is on scales that are being parameterized in present climate models, sub-1000-km scales. Only observational methods that permit derivation of gravity wave momentum fluxes over large geographical areas are discussed, and these are from satellite temperature measurements, constant-density long-duration balloons, and high-vertical-resolution radiosonde data. The models discussed include two high-resolution models in which gravity waves are explicitly modeled, Kanto and the Community Atmosphere Model, version 5 (CAM5), and three climate models containing gravity wave parameterizations, MAECHAM5, Hadley Centre Global Environmental Model 3 (HadGEM3), and the Goddard Institute for Space Studies (GISS) model. Measurements generally show similar flux magnitudes as in models, except that the fluxes derived from satellite measurements fall off more rapidly with height. This is likely due to limitations on the observable range of wavelengths, although other factors may contribute. When one accounts for this more rapid fall off, the geographical distribution of the fluxes from observations and models compare reasonably well, except for certain features that depend on the specification of the nonorographic gravity wave source functions in the climate models. For instance, both the observed fluxes and those in the high-resolution models are very small at summer high latitudes, but this is not the case for some of the climate models. This comparison between gravity wave fluxes from climate models, high-resolution models, and fluxes derived from observations indicates that such efforts offer a promising path toward improving specifications of gravity wave sources in climate models.
C1 [Geller, Marvin A.; Love, Peter T.] SUNY Stony Brook, Stony Brook, NY 11794 USA.
[Alexander, M. Joan] NorthWest Res Associates CoRA, Boulder, CO USA.
[Bacmeister, Julio] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Ern, Manfred; Preusse, Peter] Forschungszentrum Julich, D-52425 Julich, Germany.
[Hertzog, Albert] Ecole Polytech, Palaiseau, France.
[Manzini, Elisa] Max Planck Inst Meteorol, D-20146 Hamburg, Germany.
[Sato, Kaoru] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Tokyo 113, Japan.
[Scaife, Adam A.] Met Off Hadley Ctr, Exeter, Devon, England.
[Zhou, Tiehan] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Zhou, Tiehan] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
RP Geller, MA (reprint author), SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
EM marvin.geller@sunysb.edu
RI Satoh, Kaoru/P-2047-2015; Ern, Manfred/I-8839-2016; Preusse,
Peter/A-1193-2013;
OI Ern, Manfred/0000-0002-8565-2125; Preusse, Peter/0000-0002-8997-4965;
Sato, Kaoru/0000-0002-6225-6066
FU NASA Earth Science Mission Directorate [NNX08AK43G, NNH11CD32C];
National Science Foundation Climate and Large-scale Dynamics
[AGS1101258]; National Science Foundation Physical and Dynamic
Meteorology program; National Science Foundation Climate and Large-Scale
Dynamics program [0943506]; European Commission 7th Framework Programme,
COMBINE project [GA 226520]; Joint DECC/Defra Met Office Hadley Centre
Climate Programme [GA01101]; SPARC
FX Support for MAG and PTL came from the NASA Earth Science Mission
Directorate (Award NNX08AK43G) and the National Science Foundation
Climate and Large-scale Dynamics (Award AGS1101258). Support for MJA was
from the NASA Earth Science Mission Directorate (Contract NNH11CD32C)
and the National Science Foundation Physical and Dynamic Meteorology and
Climate and Large-Scale Dynamics programs (Award 0943506). EM was
partially funded by the European Commission 7th Framework Programme
under GA 226520, COMBINE project. EM is grateful to Pier Giuseppe Fogli
for technical assistance. AAS was supported by the Joint DECC/Defra Met
Office Hadley Centre Climate Programme (GA01101).; These efforts also
were motivated, in part, by the World Climate Research Programme (WCRP)
Stratospheric Processes and Their Role in Climate (SPARC) activity on
gravity waves. We thank SPARC for their help in supporting this ISSI
workshop.
NR 51
TC 85
Z9 85
U1 3
U2 53
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 SEP
PY 2013
VL 26
IS 17
BP 6383
EP 6405
DI 10.1175/JCLI-D-12-00545.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 205AK
UT WOS:000323412300011
ER
PT J
AU von Engeln, A
Teixeira, J
AF von Engeln, Axel
Teixeira, Joao
TI A Planetary Boundary Layer Height Climatology Derived from ECMWF
Reanalysis Data
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Boundary layer; Cloud cover; Climatology; Reanalysis data
ID RADIO OCCULTATION DATA; DEPTH; EVOLUTION; CYCLE
AB A planetary boundary layer (PBL) height climatology from ECMWF reanalysis data is generated and analyzed. Different methods are first compared to derive PBL heights from atmospheric temperature, pressure, and relative humidity (RH), which mostly make use of profile gradients, for example, in RH, refractivity, and virtual or potential temperature. Three methods based on the vertical gradient of RH, virtual temperature, and potential temperature were selected for the climatology generation. The RH-based method appears to capture the inversion that caps the convective boundary layer very well as a result of its temperature and humidity dependence, while the temperature-based methods appear to capture the PBL better at high latitudes. A validation of the reanalysis fields with collocated radiosonde data shows generally good agreement in terms of mean PBL height and standard deviation for the RH-based method. The generated ECMWF-based PBL height climatology shows many of the expected climatological features, such as a fairly low PBL height near the west coast of continents where stratus clouds are found and PBL growth as the air is advected over warmer waters toward the tropics along the trade winds. Large seasonal and diurnal variations are primarily found over land. The PBL height can exceed 3 km, mostly over desert areas during the day, although large values can also be found in areas such as the ITCZ. The robustness of the statistics was analyzed by using information on the percentage of outliers. Here in particular, the sea-based PBL was found to be very stable.
C1 [von Engeln, Axel] EUMETSAT, D-64295 Darmstadt, Germany.
[Teixeira, Joao] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP von Engeln, A (reprint author), EUMETSAT, Kavalleriesand 31, D-64295 Darmstadt, Germany.
EM axel.vonengeln@eumetsat.int
FU Office of Naval Research, Marine Meteorology Program [N0001411IP20087,
N0001411IP20069]; NASA MAP Program; NOAA/CPO MAPP Program; National
Aeronautics and Space Administration
FX The authors thank C. Accadia, J. Ackermann, P. Albert, T. Hewison
(EUMETSAT, Germany), and M. Schroder (DWD, Germany) for helpful
discussions, the AWI and the University of Wyoming for access to the
radiosonde data, and ECMWF for providing the different data sets used in
this study. An easy to use storage and computing environment for this
project that started in 2002 was provided by the SAT group. Special
thanks go to O. Lemke and S. Buhler (Lulea Technical University, Kiruna,
Sweden). JT acknowledges the support provided by the Office of Naval
Research, Marine Meteorology Program under Awards N0001411IP20087 and
N0001411IP20069, the NASA MAP Program, and the NOAA/CPO MAPP Program.
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. Two reviewers (D. Seidel and one
anonymous) are also acknowledged for valuable inputs.
NR 36
TC 32
Z9 32
U1 2
U2 33
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD SEP
PY 2013
VL 26
IS 17
BP 6575
EP 6590
DI 10.1175/JCLI-D-12-00385.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 205AK
UT WOS:000323412300022
ER
PT J
AU Yu, HT
Xu, F
Tropea, C
AF Yu, Haitao
Xu, Feng
Tropea, Cameron
TI Spheroidal droplet measurements based on generalized rainbow patterns
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Generalized rainbow pattern; Catastrophe optics; Airy approximation;
Geometrical optics approximation; Spheroidal droplets
ID GEOMETRICAL-OPTICS APPROXIMATION; LIGHT-SCATTERING; SPHERICAL-PARTICLES;
SIZE; CATASTROPHE; VELOCITY; FLOWS
AB The character of the rainbow from a droplet is investigated experimentally and theoretically. In the experiment, light scattering from spheroidal droplets in the vicinity of the primary rainbow region has been observed to contain a variety of characteristic interference patterns which are a generalization of the rainbow from a sphere. These patterns start from being a fold rainbow, change to transverse cusp caustics and then to hyperbolic umbilic catastrophe as the aspect ratio of the droplet increases. A comparison of the observed rainbow patterns in the horizontal equatorial plane with those of Airy theory reveals that these patterns can be used for characterizing droplet, in particular for determining the refractive index and the diameter of the droplet in the equatorial plane. The absolute error of the refractive index is smaller than 1.5 x 10(-4). The absolute relative error of the equatorial diameter is less than 5%. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Yu, Haitao; Tropea, Cameron] Tech Univ Darmstadt, Inst Fluid Mech & Aerodynam, D-64287 Darmstadt, Germany.
[Xu, Feng] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tropea, Cameron] Tech Univ Darmstadt, Ctr Smart Interfaces, D-64287 Darmstadt, Germany.
RP Yu, HT (reprint author), Tech Univ Darmstadt, Inst Fluid Mech & Aerodynam, Petersenstr 30, D-64287 Darmstadt, Germany.
EM hyu@sla.tu-darmstadt.de
RI Xu, Feng/G-3673-2013;
OI Tropea, Cameron/0000-0002-1506-9655
FU German Research Foundation [TR 194/49-1]; Graduate School Computational
Engineering and the Research Training Group GRK 1114 at the Technische
Universitat Darmstadt
FX This research is financially supported by the German Research Foundation
under Grant no. TR 194/49-1. The authors would like to thank Mr. Walter
Schafer for his useful suggestions on the experimental realization and
for many fruitful discussions. H. Yu is also grateful to the Graduate
School Computational Engineering and the Research Training Group GRK
1114 at the Technische Universitat Darmstadt for their support of his
Ph.D. program.
NR 36
TC 9
Z9 9
U1 2
U2 18
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD SEP
PY 2013
VL 126
SI SI
BP 105
EP 112
DI 10.1016/j.jqsrt.2012.09.012
PG 8
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 196US
UT WOS:000322803500016
ER
PT J
AU Mulavara, AP
Cohen, HS
Peters, BT
Sangi-Haghpeykar, H
Bloomberg, JJ
AF Mulavara, Ajitkumar P.
Cohen, Helen S.
Peters, Brian T.
Sangi-Haghpeykar, Haleh
Bloomberg, Jacob J.
TI New analyses of the sensory organization test compared to the clinical
test of sensory integration and balance in patients with benign
paroxysmal positional vertigo
SO LARYNGOSCOPE
LA English
DT Article
DE Balance testing; screening; Romberg; vestibular testing
ID DYNAMIC POSTUROGRAPHY; SUPPORT; SWAY
AB Objectives/Hypothesis To determine whether the Sensory Organization Test (SOT) of the computerized dynamic posturography battery or the Clinical Test of Sensory Integration and Balance (CTSIB) is more likely to indicate balance disorders in people with benign paroxysmal positional vertigo (BPPV).
Study Design Normal controls were compared to patients with unilateral BPPV of the posterior semicircular canal.
Methods Subjects performed tests with eyes open or closed on stable and unstable surfaces, with head still or with head moving at 0.33 Hz in pitch or yaw. Dependent variables were the percent time of the standard duration each subject could perform the task, the number of head motions made, and kinematic variables measured with head- and torso-mounted inertial motion units.
Results Because equilibrium scores of control subjects improved significantly over repeated trials on SOT, patients were given only one trial per condition. For percent time between-group differences were found on CTSIB with eyes closed, on foam, head moving in yaw showing significantly reduced performance by BPPV subjects compared to controls. Compared to controls, patients made significantly fewer head movements on CTSIB, eyes closed, on foam, head still, in pitch and yaw. Kinematic data also differed between the groups on tests with eyes closed and unstable surfaces with different head movement combinations, indicating increased instability in BPPV patients.
Conclusions For screening, CTSIB with head movements is more likely than SOT to indicate balance deficits, especially when dependent measures include percent time as well as head movement counts and kinematic measures.
C1 [Mulavara, Ajitkumar P.] Univ Space Res Assoc, Houston, TX USA.
[Cohen, Helen S.] Baylor Coll Med, Bobby R Alford Dept Otolaryngol Head & Neck Surg, Houston, TX 77030 USA.
[Sangi-Haghpeykar, Haleh] Baylor Coll Med, Dept Obstet & Gynecol, Houston, TX 77030 USA.
[Peters, Brian T.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Cohen, HS (reprint author), Baylor Coll Med, Dept Otolaryngol, 1 Baylor Plaza, Houston, TX 77030 USA.
EM hcohen@bcm.tmc.edu
FU NIH/NIDCD [1R01DC009031]; National Space Biomedical Research Institute
through NASA NCC 9-58 [SA02001]
FX Supported by NIH/NIDCD grant 1R01DC009031 (H.S.C.) and by a grant from
the National Space Biomedical Research Institute through NASA NCC 9-58
(SA02001) (A.P.M.). The authors have no other funding, financial
relationships, or conflicts of interest to disclose.
NR 18
TC 3
Z9 3
U1 6
U2 16
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0023-852X
J9 LARYNGOSCOPE
JI Laryngoscope
PD SEP
PY 2013
VL 123
IS 9
BP 2276
EP 2280
DI 10.1002/lary.24075
PG 5
WC Medicine, Research & Experimental; Otorhinolaryngology
SC Research & Experimental Medicine; Otorhinolaryngology
GA 204ZQ
UT WOS:000323410200037
PM 23553110
ER
PT J
AU Gharrett, AJ
Joyce, J
Smoker, WW
AF Gharrett, Anthony J.
Joyce, John
Smoker, William W.
TI Fine-scale temporal adaptation within a salmonid population: mechanism
and consequences
SO MOLECULAR ECOLOGY
LA English
DT Article
DE adaptation; development and evolution; ecological genetics; fish; life
history evolution
ID PINK SALMON; ONCORHYNCHUS-GORBUSCHA; LOCAL ADAPTATION; ATLANTIC SALMON;
GENETIC-VARIATION; PACIFIC SALMON; LIFE-HISTORY; FRESH-WATER; CHUM
SALMON; ALASKA
AB We demonstrate a clear example of local adaptation of seasonal timing of spawning and embryo development. The consequence is a population of pink salmon that is segmented into spawning groups that use the same limited habitat. We synthesize published observations with results of new analyses to demonstrate that genetic variation of these traits results in survival differentials related to that variation, and that density-dependent embryo mortality and seasonally variable juvenile mortality are a mechanism of selection. Most examples of local adaptation in natural systems depend on observed correlations between environments and fitness traits, but do not fully demonstrate local adaptation: that the trait is genetically determined, exhibits different fitness in common environments or across different environments, and its variation is mechanistically connected to fitness differences. The geographic or temporal scales of local adaptation often remain obscure. Here, we show that heritable, fine-scale differences of timing of reproductive migration in a pink salmon (Oncorhynchus gorbuscha) resulted in temporal structure that persisted several generations; the differences enable a density-dependent population to pack more spawners into limited spawning habitat, that is, enhance its fitness. A balanced trade-off of survivals results because embryos from early-migrating fish have a lower freshwater survival (harsh early physical conditions and disturbance by late spawners), but emigrant fry from late-migrating fish have lower marine survivals (timing of their vernal emergence into the estuarine environment). Such fine-scale local adaptations increase the genetic portfolio of the populations and may provide a buffer against the impacts of climate change.
C1 [Gharrett, Anthony J.; Joyce, John; Smoker, William W.] Univ Alaska Fairbanks, Div Fisheries, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA.
[Joyce, John] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA.
RP Gharrett, AJ (reprint author), Univ Alaska Fairbanks, Div Fisheries, Sch Fisheries & Ocean Sci, 17101 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM a.gharrett@alaska.edu
FU National Marine Fisheries Service; Alaska Sea Grant College Program
FX We thank the National Marine Fisheries Service for their support and use
of the Auke Creek facility. S. Taylor provided advice and support at the
hatchery and weir technicians M. James, J. Echave and S. Vulstek
collected samples and data. This work was supported by the Alaska Sea
Grant College Program. R. Kovach, D. Tallmon, M. Garvin, K. Palof, C.
Manhard, D. Oxman and Terrance J. Quinn provided constructive comments
on the manuscript. Thomas P. Quinn's review was helpful. References to
trade names do not imply endorsement by the National Marine Fisheries
Service, NOAA.
NR 63
TC 10
Z9 10
U1 6
U2 71
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0962-1083
EI 1365-294X
J9 MOL ECOL
JI Mol. Ecol.
PD SEP
PY 2013
VL 22
IS 17
BP 4457
EP 4469
DI 10.1111/mec.12400
PG 13
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 206GI
UT WOS:000323506400009
PM 23980763
ER
PT J
AU McCarville, DA
Guzman, JC
Sweetin, JL
Jackson, JR
Pelham, L
Steensland, J
Soden, MB
Petersen, CW
AF McCarville, D. A.
Guzman, J. C.
Sweetin, J. L.
Jackson, J. R.
Pelham, L.
Steensland, J.
Soden, M. B.
Petersen, C. W.
TI Manufacturing Overview of a 2.4 Meter (7.9 Foot) Composite Cryotank
SO SAMPE JOURNAL
LA English
DT Article
AB As part of the Space Technology Game Changing Development Program (GCDP) Composite Cryotank Technology Development (CCTD) contract, Boeing fabricated a 2.4 m diameter test article as a precursor to a 5.5 meter cryotank design, fabrication, and test. This component encompasses several challenging design features: (a) one-piece co-cured/co-bonded spherical geometry with integral skirts, (b) out-of-autoclave curing materials, (c) permeation resistant thin/hybrid ply laminate skins, and (d) thin and thick off-angle slit tape (tow) construction. The component was built on a 24 piece collapsible composite tool using robotic fiber placement. This paper details the tooling and manufacturing flow with an emphasis on process development building block activities. Lessons learned are compiled that will be used to help guide the build of a 5.5 m diameter tank during the next phase of the CCTD contract.
C1 [McCarville, D. A.; Guzman, J. C.; Sweetin, J. L.] Boeing Co, Seattle, WA USA.
[Jackson, J. R.; Pelham, L.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA.
[Steensland, J.; Soden, M. B.; Petersen, C. W.] Janicki Ind, Sedro Woolley, WA USA.
RP McCarville, DA (reprint author), Boeing Co, Seattle, WA USA.
NR 3
TC 0
Z9 0
U1 1
U2 4
PU SAMPE PUBLISHERS
PI COVINA
PA 1161 PARKVIEW DRIVE, COVINA, CA 91722 USA
SN 0091-1062
J9 SAMPE J
JI Sampe J.
PD SEP-OCT
PY 2013
VL 49
IS 5
BP 7
EP 13
PG 7
WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 207IO
UT WOS:000323592300003
ER
PT J
AU Chuang, KC
Revilock, DM
Pereira, JM
Criss, JM
Mintz, EA
AF Chuang, K. C.
Revilock, D. M.
Pereira, J. M.
Criss, J. M., Jr.
Mintz, E. A.
TI High Temperature RTM370 Polyimide Composites Fabricated by RTM:
Characterization and Impact Testing
SO SAMPE JOURNAL
LA English
DT Article
AB RTM370 imide resin based on 2,3,3;4'-biphenyl dianhydride (a-BPDA), 3,4'-oxydianiline (3,4'-ODA) and terminated with the 4-phenylethynylphthalic (PEPA) endcap has been shown to exhibit a low melt viscosity (10-30 poise) at 280 degrees C with a pot-life of 1-2 h and a high cured Tg of 370 degrees C. RTM370 resin has been successfully fabricated into composites reinforced with T650-35 carbon fabrics by resin transfer molding (RTM). RTM370 composites displays excellent mechanical properties up to 327 degrees C (620 degrees F), and outstanding property retention after aging at 288 degrees C (550 degrees F) for 1000 h, and under hot-wet conditions. RTM370 triaxial braided composites were subjected to impact test with projectiles, and exhibited enhanced energy absorption at 288 C (550 degrees F) compared to ambient temperature.
C1 [Chuang, K. C.; Revilock, D. M.; Pereira, J. M.] NASA Glenn Res Ctr, Cleveland, OH USA.
[Criss, J. M., Jr.] M&P Technol Inc, Marietta, GA USA.
[Mintz, E. A.] Clark Atlanta Univ, Atlanta, GA 30314 USA.
RP Chuang, KC (reprint author), NASA Glenn Res Ctr, Cleveland, OH USA.
EM Kathy.Chuang@nasa.gov
FU NASA Fundamental Aeronautic Supersonic Program; NASA [NCC 3-1044]
FX This work has been supported by funding from NASA Fundamental Aeronautic
Supersonic Program and NASA Cooperative Agreement to Clark Atlanta
University (NCC 3-1044). The authors also like to thank Linda S.
McCorkle for rheology measurement, photomicrographs and scanning
electron micrographs, Brian Shonkwiler for mechanical testing, Roger. R
Tokars for ultrasound scan and Daniel A. Scheiman for thermal analysis.
NR 12
TC 0
Z9 0
U1 3
U2 9
PU SAMPE PUBLISHERS
PI COVINA
PA 1161 PARKVIEW DRIVE, COVINA, CA 91722 USA
SN 0091-1062
J9 SAMPE J
JI Sampe J.
PD SEP-OCT
PY 2013
VL 49
IS 5
BP 48
EP 57
PG 10
WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 207IO
UT WOS:000323592300008
ER
PT J
AU Taylor, PT
Kis, KI
Wittmann, G
AF Taylor, P. T.
Kis, K. I.
Wittmann, G.
TI Interpretation of CHAMP magnetic anomaly data over the Pannonian Basin
region using lower altitude horizontal gradient data
SO ACTA GEODAETICA ET GEOPHYSICA
LA English
DT Article
DE SWARM; Horizontal gradient; CHAMP; Pannonian Basin
ID FIELD
AB The ESA SWARM mission will have three earth orbiting magnetometer bearing satellites one in a high orbit and two side-by-side in a lower orbit. These latter satellites will record a horizontal magnetic gradient. In order to determine how we can use these gradient measurements for interpretation of large geologic units we used ten years of CHAMP data to compute a horizontal gradient map over a section of southeastern Europe with our goal to interpret these data over the Pannonian Basin of Hungary.
C1 [Taylor, P. T.] NASA, Planetary Geodynam Lab, GSFC, Greenbelt, MD 20771 USA.
[Kis, K. I.] Eotvos Lorand Univ, Geophys & Space Sci Dept, H-1117 Budapest, Hungary.
[Wittmann, G.] MOL Hungarian Oil & Gas Co, H-1117 Budapest, Hungary.
RP Taylor, PT (reprint author), NASA, Planetary Geodynam Lab, GSFC, Greenbelt, MD 20771 USA.
EM patrick.t.taylor@nasa.gov; kisk@ludens.elte.hu; gwittmann@mol.hu
FU European Space Agency (ESA)
FX We thank the European Space Agency (ESA) for supporting the SWARM
project and especially Dr. Rune Floberghagen, Swarm Mission Manager. Dr.
Weijia Kuang reviewed our manuscript.
NR 11
TC 1
Z9 1
U1 0
U2 6
PU AKADEMIAI KIADO RT
PI BUDAPEST
PA PRIELLE K U 19, PO BOX 245,, H-1117 BUDAPEST, HUNGARY
SN 2213-5812
J9 ACTA GEOD GEOPHYS
JI Acta Geod. Geophys.
PD SEP
PY 2013
VL 48
IS 3
BP 275
EP 280
DI 10.1007/s40328-013-0026-4
PG 6
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 202MV
UT WOS:000323222300003
ER
PT J
AU Aucana, J
Llovel, W
AF Aucana, Jerome
Llovel, William
TI Deep water trends and variability at the BATS site in the subtropical
North Atlantic and consequences on local sea level budget
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE BATS time series; Sea level change; Deep water thermosteric and
halostreric effect on sea level
ID OCEAN; RISE; VENTILATION; ABYSSAL; BERMUDA; DENSITY; SERIES; HEAT
AB There is no robust evidence for warming of the global upper ocean and an associated sea-level rise based on a nearly global and continuous data coverage of the surface and upper ocean. The amount of sea level change contributed by the deep ocean is unclear, however, because of limited data availability below 2000 m. The Bermuda Atlantic Time-series Study (BATS) started monthly cruises in 1988 in the subtropical North Atlantic, and during each cruise at least one vertical profile is conducted to a depth >4000 m. The BATS dataset provides a unique estimation of the seasonal to inter-annual hydrographic variability in the deep ocean as well as long-term trends at a fixed location. In this paper, we focus on the 2000-4000 m deep layer, and find (1) an isopycnal cooling and freshening trend in the deep subtropical North Atlantic, (2) an isobaric warming since similar to year 2000, despite the continued isopycnal cooling, driven by a gradual deepening of neutral surfaces with unknown spatial extent, and (3) a previously undocumented high frequency variability (>1 yr(-1)) of the deep ocean characterized by large (100 m) episodic vertical displacements of neutral surfaces. The observed water mass changes below 2000 m contribute similar to 1 mm/yr to the 0-4000 m steric height budget, and is driven mainly by the halos teric contribution. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Aucana, Jerome] IRD LEGOS, F-31400 Toulouse, France.
[Llovel, William] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Aucana, J (reprint author), IRD LEGOS, 14 Ave Edouard Belin, F-31400 Toulouse, France.
EM jerome.aucan@ird.fr
RI Aucan, Jerome/M-8378-2014; LLOVEL, William/G-6930-2016
OI Aucan, Jerome/0000-0002-9883-0082;
FU NSF [OCE 88-01089, OCE 93-01950, OCE 96-17795 OCE-0326885]; Oak Ridge
Associated Universities through the NASA Postdoctoral Program (NPP)
FX Insightful discussions with Benoit Meyssignac helped improve the scope
of this paper. Financial support for BATS has come largely from NSF
(primarily OCE 88-01089,OCE 93-01950, OCE 96-17795 OCE-0326885). William
Llovel was supported by Oak Ridge Associated Universities through the
NASA Postdoctoral Program (NPP) and carried out by the Jet Propulsion
Laboratory, California Institute of Technology.
NR 32
TC 0
Z9 0
U1 0
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
EI 1879-0100
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD SEP
PY 2013
VL 93
SI SI
BP 169
EP 176
DI 10.1016/j.dsr2.2013.01.003
PG 8
WC Oceanography
SC Oceanography
GA 202BT
UT WOS:000323189200014
ER
PT J
AU Brady, AL
Druschel, G
Leoni, L
Lim, DSS
Slater, GF
AF Brady, A. L.
Druschel, G.
Leoni, L.
Lim, D. S. S.
Slater, G. F.
TI Isotopic biosignatures in carbonate-rich, cyanobacteria-dominated
microbial mats of the Cariboo Plateau, BC
SO GEOBIOLOGY
LA English
DT Review
ID SULFATE-REDUCING BACTERIA; FRESH-WATER MICROBIALITES; DISSOLVED
INORGANIC CARBON; YELLOWSTONE-NATIONAL-PARK; SOLAR LAKE SINAI;
FATTY-ACID COMPOSITION; BLUE-GREEN-ALGAE; ORGANIC-CARBON;
BRITISH-COLUMBIA; BIOLOGICAL CARBONATES
AB Photosynthetic activity in carbonate-rich benthic microbial mats located in saline, alkaline lakes on the Cariboo Plateau, B.C. resulted in pCO(2) below equilibrium and C-13(DIC) values up to +6.0 parts per thousand above predicted carbon dioxide (CO2) equilibrium values, representing a biosignature of photosynthesis. Mat-associated C-13(carb) values ranged from similar to 4 to 8 parts per thousand within any individual lake, with observations of both enrichments (up to 3.8 parts per thousand) and depletions (up to 11.6 parts per thousand) relative to the concurrent dissolved inorganic carbon (DIC). Seasonal and annual variations in C-13 values reflected the balance between photosynthetic C-13-enrichment and heterotrophic inputs of C-13-depleted DIC. Mat microelectrode profiles identified oxic zones where C-13(carb) was within 0.2 parts per thousand of surface DIC overlying anoxic zones associated with sulphate reduction where C-13(carb) was depleted by up to 5 parts per thousand relative to surface DIC reflecting inputs of C-13-depleted DIC. C-13 values of sulphate reducing bacteria biomarker phospholipid fatty acids (PLFA) were depleted relative to the bulk organic matter by similar to 4 parts per thousand, consistent with heterotrophic synthesis, while the majority of PLFA had larger offsets consistent with autotrophy. Mean C-13(org) values ranged from -18.7 +/- 0.1 to -25.3 +/- 1.0 parts per thousand with mean C-13(inorg-org) values ranging from 21.1 to 24.2 parts per thousand, consistent with non-CO2-limited photosynthesis, suggesting that Precambrian C-13(org) values of similar to-26 parts per thousand do not necessitate higher atmospheric CO2 concentrations. Rather, it is likely that the high DIC and carbonate content of these systems provide a non-limiting carbon source allowing for expression of large photosynthetic offsets, in contrast to the smaller offsets observed in saline, organic-rich and hot spring microbial mats.
C1 [Brady, A. L.; Leoni, L.; Slater, G. F.] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON, Canada.
[Druschel, G.] Indiana Univ Purdue Univ, Dept Earth Sci, Indianapolis, IN 46202 USA.
[Lim, D. S. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Lim, D. S. S.] SETI Inst, Mountain View, CA USA.
RP Slater, GF (reprint author), McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON, Canada.
EM gslater@mcmaster.ca
FU Natural Sciences and Engineering Research Council of Canada (NSERC); CSA
CARN program; NSERC
FX Infrastructure support for our field research was provided by a Canadian
Space Agency (CSA) Canadian Analogue Research Network (CARN) PLRP
contract. Funding was provided by a Natural Sciences and Engineering
Research Council of Canada (NSERC) Discovery Grant to G. F. S. and the
CSA CARN program with partial support from an NSERC Post-Graduate
Scholarship to A. L. B. Thank you to Jennie Kirby, Martin Knyf, Jen
Hansen, Matt Johnston and members of the Environmental Organic
Geochemistry Laboratory at McMaster University for valuable lab
assistance and to all of the PLRP support staff.
NR 130
TC 5
Z9 5
U1 1
U2 28
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 SEP
PY 2013
VL 11
IS 5
BP 437
EP 456
DI 10.1111/gbi.12050
PG 20
WC Biology; Environmental Sciences; Geosciences, Multidisciplinary
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Geology
GA 200OL
UT WOS:000323078400005
PM 23941467
ER
PT J
AU Narkawicz, A
Munoz, C
Herencia-Zapana, H
Hagen, G
AF Narkawicz, Anthony
Munoz, Cesar
Herencia-Zapana, Heber
Hagen, George
TI Formal verification of lateral and temporal safety buffers for
state-based conflict detection
SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART G-JOURNAL OF
AEROSPACE ENGINEERING
LA English
DT Article
DE Formal verification; air traffic management; aircraft conflict
resolution
AB This article presents an analytical definition of lateral and temporal safety buffers to be used in state-based conflict detection algorithms. A lateral buffer is a distance to be added to the minimum lateral separation to accommodate for uncertainty in the surveillance information. A temporal buffer is a time to be added to the lookahead conflict detection time to accommodate for dropped surveillance messages due to signal attenuation. These safety buffers are defined using precise mathematical statements and the main theorems give numerical upper bounds on the probability of a missed alert. A particular case is considered where absolute bounds on the errors in position and velocity information are known. In this case, under well-defined assumptions provided in this article, safety buffers are given that guarantee mathematically that the probability of a missed alert is zero. The results are presented as theorems, which were formally proven using a mechanical theorem prover.
C1 [Narkawicz, Anthony; Munoz, Cesar; Hagen, George] NASA, Langley Res Ctr, Washington, DC USA.
[Herencia-Zapana, Heber] Natl Inst Aerosp, Hampton, VA 23666 USA.
RP Herencia-Zapana, H (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA.
EM heber.herencia-zapana@nianet.org
FU National Aeronautics and Space Administration [NCC-1-02043]
FX Heber Herencia-Zapana was supported by the National Aeronautics and
Space Administration under NASA Cooperative Agreement NCC-1-02043.
NR 26
TC 0
Z9 0
U1 2
U2 5
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0954-4100
J9 P I MECH ENG G-J AER
JI Proc. Inst. Mech. Eng. Part G-J. Aerosp. Eng.
PD SEP
PY 2013
VL 227
IS 9
BP 1412
EP 1424
DI 10.1177/0954410012456495
PG 13
WC Engineering, Aerospace; Engineering, Mechanical
SC Engineering
GA 196JZ
UT WOS:000322772200003
ER
PT J
AU Healy, AF
Schneider, VI
McCormick, B
Fierman, DM
Buck-Gengler, CJ
Barshi, I
AF Healy, Alice F.
Schneider, Vivian I.
McCormick, Blu
Fierman, Deanna M.
Buck-Gengler, Carolyn J.
Barshi, Immanuel
TI Which modality is best for presenting navigation instructions?
SO JOURNAL OF APPLIED RESEARCH IN MEMORY AND COGNITION
LA English
DT Article
DE Modality; Navigation instructions; Multiple resources; Memory
AB experiments involved college students receiving and following instructions of various lengths for navigating in a three-dimensional space displayed on a computer screen. The purpose was to evaluate which is the best modality for presenting navigation instructions so that they can be executed successfully. Single modalities (read, hear, and see) were considered along with dual modalities presented simultaneously or successively. It was found that when there were differences between single modalities, generally execution accuracy was best for see and worst for read. Information presented in two modalities did not yield better accuracy than information presented twice in a single modality. Also, the ordering of modalities depended on the extent of practice. Thus, presentation modality does not have a consistently large effect on receiving and following navigation instructions. Repetition and the amount of practice are much more important variables than is presentation modality in determining how well navigation instructions are followed. (C) 2013 Society for Applied Research in Memory and Cognition. Published by Elsevier Inc. All rights reserved.
C1 [Healy, Alice F.; Schneider, Vivian I.; McCormick, Blu; Fierman, Deanna M.; Buck-Gengler, Carolyn J.] Univ Colorado, Dept Psychol & Neurosci, Boulder, CO 80309 USA.
[Barshi, Immanuel] NASA, Ames Res Ctr, Human Syst Integrat Div, Washington, DC USA.
RP Healy, AF (reprint author), Univ Colorado, Dept Psychol & Neurosci, Muen Zinger Bldg,345 UCB, Boulder, CO 80309 USA.
EM alice.healy@colorado.edu
FU National Aeronautics and Space Administration Grant [NNA05CS42A,
NNA07CN59A, NNX10AC87A]; Army Research Institute [DASW01-03-K-0002];
Army Research Office Grant [W911NF-05-1-0153]
FX This research was supported in part by National Aeronautics and Space
Administration Grants NNA05CS42A, NNA07CN59A, and NNX10AC87A, Army
Research Institute Contract DASW01-03-K-0002, and Army Research Office
Grant W911NF-05-1-0153 to the University of Colorado. A preliminary
version of Experiment 1 was presented at the Symposium on Memory
Dynamics and the Optimization of Instruction at the 2007 annual
convention of the American Psychological Association, a preliminary
version of Experiment 2 was presented at the 2008 annual meeting of the
Psychonomic Society, and all three experiments were reviewed at the 2013
biennial meeting of the Society for Applied Research in Memory and
Cognition. We would like to thank Lyle Bourne for thoughtful suggestions
and advice concerning this research.
NR 35
TC 3
Z9 3
U1 1
U2 2
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 2211-3681
EI 2211-369X
J9 J APPL RES MEM COGN
JI J. Appl. Res. Mem. Cogn.
PD SEP
PY 2013
VL 2
IS 3
BP 192
EP 199
DI 10.1016/j.jarmac.2013.07.004
PG 8
WC Psychology, Experimental
SC Psychology
GA V38TK
UT WOS:000209365500008
ER
PT J
AU King, A
Lakhani, KR
AF King, Andrew
Lakhani, Karim R.
TI Using Open Innovation to Identity the Best Ideas
SO MIT SLOAN MANAGEMENT REVIEW
LA English
DT Article
C1 [King, Andrew] Dartmouth Coll, Tuck Sch Business, Hanover, NH 03755 USA.
[Lakhani, Karim R.] Harvard Univ, Sch Business, Cambridge, MA 02138 USA.
[Lakhani, Karim R.] NASA, Tournament Lab, Washington, DC USA.
RP King, A (reprint author), Dartmouth Coll, Tuck Sch Business, Hanover, NH 03755 USA.
EM smrfeedback@mit.edu; smrfeedback@mit.edu
NR 14
TC 13
Z9 13
U1 5
U2 15
PU SLOAN MANAGEMENT REVIEW ASSOC, MIT SLOAN SCHOOL MANAGEMENT
PI CAMBRIDGE
PA 77 MASSACHUSETTS AVE, E60-100, CAMBRIDGE, MA 02139-4307 USA
SN 1532-9194
J9 MIT SLOAN MANAGE REV
JI MIT Sloan Manage. Rev.
PD FAL
PY 2013
VL 55
IS 1
BP 41
EP 48
PG 8
WC Business; Management
SC Business & Economics
GA V37MP
UT WOS:000209280200010
ER
PT J
AU Tadesse, T
Wiegelmann, T
MacNeice, PJ
Olson, K
AF Tadesse, Tilaye
Wiegelmann, T.
MacNeice, P. J.
Olson, K.
TI Modeling coronal magnetic field using spherical geometry: cases with
several active regions
SO ASTROPHYSICS AND SPACE SCIENCE
LA English
DT Article
DE Active regions: magnetic fields; Active regions: models; Magnetic
fields: corona; Magnetic fields: photosphere; Magnetic fields: models
ID FORCE-FREE FIELDS; SOLAR CORONA; RECONSTRUCTION; EXTRAPOLATION
AB The magnetic fields in the solar atmosphere structure the plasma, store free magnetic energy and produce a wide variety of active solar phenomena, like flare and coronal mass ejections (CMEs). The distribution and strength of magnetic fields are routinely measured in the solar surface (photosphere). Therefore, there is considerable interest in accurately modeling the 3D structure of the coronal magnetic field using photospheric vector magnetograms. Knowledge of the 3D structure of magnetic field lines also help us to interpret other coronal observations, e.g., EUV images of the radiating coronal plasma. Nonlinear force-free field (NLFFF) models are thought to be viable tools for those task. Usually those models use Cartesian geometry. However, the spherical nature of the solar surface cannot be neglected when the field of view is large. In this work, we model the coronal magnetic field above multiple active regions using NLFFF extrapolation code using vector magnetograph data from the Synoptic Optical Long-term Investigations of the Sun survey (SOLIS)/Vector Spectromagnetograph (VSM) as a boundary conditions. We compare projections of the resulting magnetic field lines solutions with their respective coronal EUV-images from the Atmospheric Imaging Assembly (SDO/AIA) observed on October 15, 2011 and November 13, 2012. This study has found that the NLFFF model in spherical geometry reconstructs the magnetic configurations for several active regions which agrees to some extent with observations. During October 15, 2011 observation, there are substantial number of trans-equatorial loops carrying electric current.
C1 [Tadesse, Tilaye; MacNeice, P. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wiegelmann, T.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Olson, K.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA.
RP Tadesse, T (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA.
EM tilaye.tadesse.asfaw@nasa.gov
FU NASA
FX SOLIS/VSM vector magnetograms are produced cooperatively by NSF/NSO and
NASA/LWS. The National Solar Observatory (NSO) is operated by the
Association of Universities for Research in Astronomy, Inc., under
cooperative agreement with the National Science Foundation. This
research was supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center (GSFC), administered by Oak
Ridge Associated Universities through a contract with NASA.
NR 27
TC 4
Z9 4
U1 2
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0004-640X
J9 ASTROPHYS SPACE SCI
JI Astrophys. Space Sci.
PD SEP
PY 2013
VL 347
IS 1
BP 21
EP 27
DI 10.1007/s10509-013-1493-3
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 193QL
UT WOS:000322576100003
ER
PT J
AU Weiss, S
Achtelik, MW
Lynen, S
Achtelik, MC
Kneip, L
Chli, M
Siegwart, R
AF Weiss, Stephan
Achtelik, Markus W.
Lynen, Simon
Achtelik, Michael C.
Kneip, Laurent
Chli, Margarita
Siegwart, Roland
TI Monocular Vision for Long-term Micro Aerial Vehicle State Estimation: A
Compendium
SO JOURNAL OF FIELD ROBOTICS
LA English
DT Article
ID OBSERVABILITY ANALYSIS; FUSION; CALIBRATION; MOTION; ENVIRONMENTS;
NAVIGATION; SLAM
AB The recent technological advances in Micro Aerial Vehicles (MAVs) have triggered great interest in the robotics community, as their deployability in missions of surveillance and reconnaissance has now become a realistic prospect. The state of the art, however, still lacks solutions that can work for a long duration in large, unknown, and GPS-denied environments. Here, we present our visual pipeline and MAV state-estimation framework, which uses feeds from a monocular camera and an Inertial Measurement Unit (IMU) to achieve real-time and onboard autonomous flight in general and realistic scenarios. The challenge lies in dealing with the power and weight restrictions onboard a MAV while providing the robustness necessary in real and long-term missions. This article provides a concise summary of our work on achieving the first onboard vision-based power-on-and-go system for autonomous MAV flights. We discuss our insights on the lessons learned throughout the different stages of this research, from the conception of the idea to the thorough theoretical analysis of the proposed framework and, finally, the real-world implementation and deployment. Looking into the onboard estimation of monocular visual odometry, the sensor fusion strategy, the state estimation and self-calibration of the system, and finally some implementation issues, the reader is guided through the different modules comprising our framework. The validity and power of this framework are illustrated via a comprehensive set of experiments in a large outdoor mission, demonstrating successful operation over flights of more than 360m trajectory and 70m altitude change.(1) (C) 2013 Wiley Periodicals, Inc.
C1 [Weiss, Stephan; Achtelik, Markus W.; Lynen, Simon] CALTECH, NASA, JPL, Pasadena, CA 91125 USA.
[Weiss, Stephan; Achtelik, Markus W.; Lynen, Simon; Kneip, Laurent; Chli, Margarita; Siegwart, Roland] Swiss Fed Inst Technol, Autonomous Syst Lab, Zurich, Switzerland.
RP Weiss, S (reprint author), CALTECH, NASA, JPL, Pasadena, CA 91125 USA.
EM stephan.weiss@ieee.org; markus.achtelik@mavt.ethz.ch;
simon.lynen@mavt.ethz.ch; michael.achtelik@asctec.de;
laurent.kneip@mavt.ethz.ch; mar-garita.chli@mavt.ethz.ch;
r.siegwart@ieee.org
RI Siegwart, Roland/A-4495-2008;
OI Siegwart, Roland/0000-0002-2760-7983; Kneip, Laurent/0000-0001-6727-6608
FU European Community [231855, 266470, 285417]
FX The research leading to this article has received funding from the
European Community's Seventh Framework Program (FP7/2007-2013) under
grant agreements no. 231855 (www.sfly.org), no. 266470
(www.mycopter.eu), and no. 285417 (www.fp7-icarus.eu). Stephan Weiss is
technologist at NASA-JPL/CalTech (email: stephan.weiss@ieee.org). Markus
W. Achtelik, Simon Lynen and Laurent Kneip are currently Ph.D. students
at the ETH Zurich (email: "markus.achtelik, simon.lynen, laurent.kneip"
@mavt.ethz.ch). Michael C. Achtelik is CEO of Ascending Technologies
GmbH (email: michael.achtelik@asctec.de). Margarita Chli is a senior
researcher at and deputy director of the Autonomous Systems Lab (ASL) at
ETH Zurich (email: margarita.chli@mavt.ethz.ch). Roland Siegwart is full
professor at the ETH Zurich and head of the ASL (email:
r.siegwart@ieee.org).
NR 72
TC 63
Z9 65
U1 10
U2 41
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1556-4959
EI 1556-4967
J9 J FIELD ROBOT
JI J. Field Robot.
PD SEP
PY 2013
VL 30
IS 5
BP 803
EP 831
DI 10.1002/rob.21466
PG 29
WC Robotics
SC Robotics
GA 196GI
UT WOS:000322761100008
ER
PT J
AU Evirgen, A
Karaman, I
Noebe, RD
Santamarta, R
Pons, J
AF Evirgen, A.
Karaman, I.
Noebe, R. D.
Santamarta, R.
Pons, J.
TI Effect of precipitation on the microstructure and the shape memory
response of the Ni50.3Ti29.7Zr20 high temperature shape memory alloy
SO SCRIPTA MATERIALIA
LA English
DT Article
DE High temperature shape memory alloys; Shape memory response;
Precipitation; Martensitic transformation; NiTiZr
ID ZR; BEHAVIOR
AB The effect of nano-precipitation on the shape memory characteristics and martensite microstructure of the Ni50.3Ti29.7Zr20 high temperature shape memory alloy was studied. With appropriate heat treatment, the alloy shows excellent dimensional stability during thermal cycling under tension. Fine precipitates are absorbed by martensite variants and do not significantly hinder martensite formation. These alloys demonstrated higher transformation strain, smaller thermal hysteresis and narrower transformation range than samples with larger precipitates, a few hundred nanometers, that interfere with martensite variant growth. (c) 2013 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Evirgen, A.; Karaman, I.] Texas A&M Univ, Mat Sci & Engn Grad Program, College Stn, TX 77843 USA.
[Karaman, I.] Texas A&M Univ, Dept Mech Engn, College Stn, TX 77843 USA.
[Noebe, R. D.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Santamarta, R.; Pons, J.] Univ Illes Balears, Dept Fis, E-07122 Palma de Mallorca, Spain.
RP Karaman, I (reprint author), Texas A&M Univ, Mat Sci & Engn Grad Program, College Stn, TX 77843 USA.
EM ikaraman@tamu.edu
RI Karaman, Ibrahim/E-7450-2010; Santamarta, Ruben/K-7865-2016
OI Karaman, Ibrahim/0000-0001-6461-4958; Santamarta,
Ruben/0000-0003-3341-5758
FU US Air Force Office of Scientific Research [FA9550-12-1-0218]; Spanish
MINECO; FEDER [MAT2011-28217-C02-01]; NASA Fundamental Aeronautics
Program, Aeronautical Sciences Project
FX This work was supported by the US Air Force Office of Scientific
Research, Grant no. FA9550-12-1-0218. Partial financial support from
Spanish MINECO and FEDER under project number MAT2011-28217-C02-01 is
acknowledged. R.D.N. gratefully acknowledges support from the NASA
Fundamental Aeronautics Program, Aeronautical Sciences Project.
NR 13
TC 19
Z9 19
U1 2
U2 26
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6462
J9 SCRIPTA MATER
JI Scr. Mater.
PD SEP
PY 2013
VL 69
IS 5
BP 354
EP 357
DI 10.1016/j.scriptamat.2013.05.006
PG 4
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 191MF
UT WOS:000322416500003
ER
PT J
AU Ainley, DG
Nur, N
Eastman, JT
Ballard, G
Parkinson, CL
Evans, CW
DeVries, AL
AF Ainley, David G.
Nur, Nadav
Eastman, Joseph T.
Ballard, Grant
Parkinson, Claire L.
Evans, Clive W.
DeVries, Arthur L.
TI Decadal trends in abundance, size and condition of Antarctic toothfish
in McMurdo Sound, Antarctica, 1972-2011
SO FISH AND FISHERIES
LA English
DT Article
DE Antarctic toothfish; Antarctic silverfish; climate change; change in
fish condition; change in fish abundance; sea-ice; Ross Sea; Southern
Ocean
ID DISSOSTICHUS-MAWSONI PERCIFORMES; EARLY-LIFE STAGES; ROSS SEA SHELF;
SOUTHERN-OCEAN; PLEURAGRAMMA-ANTARCTICUM; MANAGING FISHERIES; MARINE
ECOSYSTEMS; POPULATION-CHANGE; PACIFIC SECTOR; WEDDELL SEALS
AB We report the analyses of a dataset spanning 39years of near-annual fishing for Dissostichus mawsoni in McMurdo Sound, Antarctica, 1972-2011. Data on total length, condition and catch per unit effort (CPUE) were derived from the>5500 fish caught, the large majority of which were measured, tagged and released. Contrary to expectation, the length frequency of the McMurdo Sound catch was dominated by fish in the upper two-thirds of the overall distribution exhibited in the industrial catch for the Ross Sea shelf. Fish length and condition increased from the early 1970s to the early 1990s and then decreased. Fish length positively correlated with Ross Sea ice extent in early spring, a relationship possibly caused by more ice encouraging larger fish to move farther south over the shelf and into the study area. Fish condition positively correlated with the amount of open water in the Ross Sea during the previous summer (Feb), perhaps reflecting greater availability of prey with the higher productivity that more open water brings. Decreasing fish size corresponds to the onset of the fishery, which targets the large individuals. CPUE was constant through 2001 and then decreased dramatically. We hypothesize that this decrease is related to the industrial fishery, which began in the 1996-97 austral summer, and concentrates effort over the ice-free Ross Sea continental slope. As a result of limited prey choices and close coupling among mesopredators of the region, Antarctic toothfish included, the fishery appears to be dramatically altering the trophic structure of the Ross Sea.
C1 [Ainley, David G.] HT Harvey & Associates, Los Gatos, CA 95032 USA.
[Nur, Nadav; Ballard, Grant] PRBO Conservat Sci, Petaluma, CA 94954 USA.
[Eastman, Joseph T.] Ohio Univ, Coll Osteopath Med, Dept Biomed Sci, Athens, OH 45701 USA.
[Parkinson, Claire L.] NASA, Cryospher Sci Lab, Code 615, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Evans, Clive W.] Univ Auckland, Sch Biol Sci, Auckland 1, New Zealand.
[DeVries, Arthur L.] Univ Illinois, Dept Anim Biol, Urbana, IL 61801 USA.
RP Ainley, DG (reprint author), HT Harvey & Associates, Los Gatos, CA 95032 USA.
EM dainley@penguinscience.com
RI Eastman, Joseph/A-9786-2008; Parkinson, Claire/E-1747-2012
OI Parkinson, Claire/0000-0001-6730-4197
FU US National Science Foundation; Lenfest Ocean Program; NSF Office of
Polar Programs [ANT-0440643]
FX The fishing effort described was funded for most of its tenure by the US
National Science Foundation; logistics support was provided by the US
Antarctic Program and Antarctica NZ. Data analysis and writing were
funded by the Lenfest Ocean Program, and by the NSF Office of Polar
Programs, Grant ANT-0440643. The data set is now archived by CCAMLR. The
views expressed herein do not necessarily reflect those of the National
Science Foundation, and we have no conflicts of interest. We appreciate
comments on the manuscript by C. Brooks, S. Hanchet, M. Pinkerton, J.
Rotella, D. Siniff and D. Zajanc; all improved it significantly. PRBO
contribution # 1866.
NR 81
TC 12
Z9 12
U1 4
U2 53
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1467-2960
J9 FISH FISH
JI Fish. Fish.
PD SEP
PY 2013
VL 14
IS 3
BP 343
EP 363
DI 10.1111/j.1467-2979.2012.00474.x
PG 21
WC Fisheries
SC Fisheries
GA 185ZW
UT WOS:000322011800007
ER
PT J
AU Garcia-Ricard, OJ
Meza-Morales, P
Silva-Martinez, JC
Curet-Arana, MC
Hogan, JA
Hernandez-Maldonado, AJ
AF Garcia-Ricard, Omar J.
Meza-Morales, Paul
Silva-Martinez, Juan C.
Curet-Arana, Maria C.
Hogan, John A.
Hernandez-Maldonado, Arturo J.
TI Carbon dioxide storage and sustained delivery by Cu-2(pzdc)(2)L [L =
dipyridyl-based ligand] pillared-layer porous coordination networks
SO MICROPOROUS AND MESOPOROUS MATERIALS
LA English
DT Article
DE Porous coordination polymers; Metal-organic frameworks; Pillared-layer
structure; Carbon dioxide storage; Carbon dioxide delivery
ID METAL-ORGANIC FRAMEWORKS; MOLECULAR ELECTROSTATIC POTENTIALS; ZEOLITIC
IMIDAZOLATE FRAMEWORKS; ACTIVATION TEMPERATURE; TEXTURAL PROPERTIES; CO2
ADSORPTION; GAS-STORAGE; DENSITY; ZIF-8
AB CPL-2 (Cu-2(pzdc)(2)(bpy)), CPL-5 ((Cu-2(pzdc)(2)(bpe)), and ZIF-8 (Zn(MelM)(2)) [pzdc = 2,3-pyrazinedicarboxylate, bpy = 4,4'bipyridine, bpe = 1,2-di-(4-pyridyl)-ethylene, MeIM = 2-methylimidazolate] were used to study carbon dioxide storage and delivery at low to moderate pressures. Both CPL-2 and CPL-5 showed superior performance over ZIF-8 due to better volumetric-based capacities and superior diffusion kinetics exhibited by the former metal organic frameworks. When compared with an empty vessel, the CPL-n based storage/delivery system provided as much as 500% increase in CO2 constant flow supply time at moderate pressures. A simplified phenomenological yet useful model was developed to predict discharge pressure decay and estimate a lumped parameter related to the molecular diffusivity. Density functional theory was also employed to shed light onto the CO2 hysteretic adsorption process present on the CPL-n materials. Greater CO2 binding interactions were observed near the vicinity of the copper-nodes. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Garcia-Ricard, Omar J.; Meza-Morales, Paul; Silva-Martinez, Juan C.; Curet-Arana, Maria C.; Hernandez-Maldonado, Arturo J.] Univ Puerto Rico, Dept Chem Engn, Mayaguez, PR 00681 USA.
[Hogan, John A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Hernandez-Maldonado, AJ (reprint author), Univ Puerto Rico, Dept Chem Engn, Mayaguez Campus, Mayaguez, PR 00681 USA.
EM arturoj.hernandez@upr.edu
FU National Aeronautics and Space Administration (NASA) [NNX13AD38A]; NASA
Graduate Student Research Project Award [NNX10AL59H]; National Science
Foundation (NSF) Partnership for Research and Education in Materials
Award [DMR-0934115]; Puerto Rico Institute for Functional Materials
under the NSF [EPS-1002410]
FX Support was provided by the National Aeronautics and Space
Administration (NASA) Award NNX13AD38A and NASA Graduate Student
Research Project Award NNX10AL59H. The computational work was supported
by the National Science Foundation (NSF) Partnership for Research and
Education in Materials Award DMR-0934115. and the Puerto Rico Institute
for Functional Materials under the NSF Award EPS-1002410.
NR 32
TC 6
Z9 6
U1 3
U2 53
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1387-1811
J9 MICROPOR MESOPOR MAT
JI Microporous Mesoporous Mat.
PD SEP 1
PY 2013
VL 177
BP 54
EP 58
DI 10.1016/j.micromeso.2013.04.018
PG 5
WC Chemistry, Applied; Chemistry, Physical; Nanoscience & Nanotechnology;
Materials Science, Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA 189UE
UT WOS:000322293000010
ER
PT J
AU Banks, JR
Brindley, HE
Flamant, C
Garay, MJ
Hsu, NC
Kalashnikov, OV
Kluser, L
Sayer, AM
AF Banks, J. R.
Brindley, H. E.
Flamant, C.
Garay, M. J.
Hsu, N. C.
Kalashnikov, O. V.
Klueser, L.
Sayer, A. M.
TI Intercomparison of satellite dust retrieval products over the west
African Sahara during the Fennec campaign in June 2011
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Remote sensing of dust; Satellite retrieval intercomparisons; Aerosol
optical depth; Fennec
ID INFRARED EXTINCTION SPECTRA; OPTICAL DEPTH RETRIEVALS; MINERAL DUST;
AEROSOL PROPERTIES; MISR AEROSOL; NORTH-AFRICA; DESERT; AERONET; LAND;
INSTRUMENT
AB Four aerosol optical depth retrieval algorithms over the Sahara Desert during June 2011 from the IASI, MISR,. MODIS, and SEVIRI satellite instruments are compared against each other in order to understand the strengths and weaknesses of each retrieval approach. Particular attention is paid to the effects of meteorological conditions, land surface properties, and the magnitude of the dust loading. The period of study corresponds to the time of the first Fennec intensive measurement campaign, which provides new ground-based and aircraft measurements of the dust characteristics and loading. Validation using ground-based AERONET sunphotometer data indicates that of the satellite products, the SEVIRI retrieval is most able to retrieve dust during optically thick dust events, whereas IASI and MODIS perform better at low dust loadings. This may significantly affect observations of dust emission and the mean dust climatology. MISR and MODIS are least sensitive to variations in meteorological conditions, while SEVIRI tends to overestimate the aerosol optical depth (AOD) under moist conditions (with a bias against AERONET of 0.31), especially at low dust loadings where the AOD < 1. Further comparisons are made with airborne LIDAR measurements taken during the Fennec campaign, which provide further evidence for the inferences made from the AERONET comparisons. The effect of surface properties on the retrievals is also investigated. Over elevated surfaces IASI retrieves AODs which are most consistent with AERONET observations, while the AODs retrieved by MODIS tend to be biased low. In contrast, over the least emissive surfaces IASI significantly underestimates the AOD (with a bias of -0.41), while MISR and SEVIRI show closest agreement. (C) 2013 The Authors. Published by Elsevier Inc. All rights reserved.
C1 [Banks, J. R.; Brindley, H. E.] Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, London SW7 2BW, England.
[Flamant, C.] CNRS, UMR 8190, Lab Atmospheres, Paris, France.
[Garay, M. J.; Kalashnikov, O. V.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Hsu, N. C.; Sayer, A. M.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Klueser, L.] German Remote Sensing Datactr DFD, German Aerosp Ctr DLR, D-82334 Wessling, Germany.
[Sayer, A. M.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res GESTAR, Columbia, MD USA.
RP Banks, JR (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Space & Atmospher Phys Grp, Prince Consort Rd, London SW7 2BW, England.
EM j.banks@imperial.ac.uk
RI Sayer, Andrew/H-2314-2012;
OI Sayer, Andrew/0000-0001-9149-1789; Banks, James/0000-0002-6701-7144;
Brindley, Helen/0000-0002-7859-9207
FU Agence Nationale de la Recherche (ANR); Institut National des Sciences
de l'Univers (INSU/CNRS) through the LEFE program; Centre National
d'Etudes Spatiales (CNES) through the TOSCA program; Meteo-France; UK
Natural Environment Research Council [NE/G016283/1]; National
Aeronautics and Space Administration
FX We thank the AERONET PIs and staff for establishing and maintaining the
nine sites used in this study; the Fennec supersites at BBM and Zouerat
were operated by the Offices Nationals de la Meteorologie (ONM) of
Algeria and Mauritania. The ERA-Interim meteorological data were
produced by ECWMF, and access to the dataset was provided by the British
Atmospheric Data Centre. Thanks also go to the Royal Meteorological
Institute of Belgium for the provision of surface elevation and albedo
dataand also 'GERBlike' data used in the SEVIRI AOD retrieval, as well
as to researchers at the Cooperative Institute for Meteorological
Satellite Studies at the University of Wisconsin for the emissivity
data. This work has been carried out as part of the Fennec project. The
Fennec-France project is funded by the Agence Nationale de la Recherche
(ANR), the Institut National des Sciences de l'Univers (INSU/CNRS)
through the LEFE program, by the Centre National d'Etudes Spatiales
(CNES) through the TOSCA program and by Meteo-France. Many thanks to the
SAFIRE team for the radiation and dropsonde data from the Falcon 20 as
well as to J. Pelon (LATMOS). The authors are grateful to D. Bruneau and
P. Genau (LATMOS), F. Blouzon and A. Abchiche (DT/INSU) for operating
the LNG system in the Falcon 20. The work of M. Garay and O.
Kalashnikova was carried out at the Jet Propulsion Laboratory,
California Institute of Technology under a contract with the National
Aeronautics and Space Administration. Thanks also to John Marsham at the
University of Leeds for his helpful comments during the preparation of
this work, and to two anonymous reviewers whose valuable comments have
also improved this work. J. R. Banks is supported under grant
NE/G016283/1 by the UK Natural Environment Research Council.
NR 75
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Z9 25
U1 1
U2 35
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2013
VL 136
BP 99
EP 116
DI 10.1016/j.rse.2013.05.003
PG 18
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 186PC
UT WOS:000322055600010
ER
PT J
AU van Leeuwen, M
Coops, NC
Hilker, T
Wulder, MA
Newnham, GJ
Culvenor, DS
AF van Leeuwen, Martin
Coops, Nicholas C.
Hilker, Thomas
Wulder, Michael A.
Newnham, Glenn J.
Culvenor, Darius S.
TI Automated reconstruction of tree and canopy structure for modeling the
internal canopy radiation regime
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Laser scanning; Canopy structure; Photosynthetically active radiation;
Explicit geometric; Modeling; Ray tracing
ID GROUND-BASED LIDAR; FOREST CANOPIES; SURFACE RECONSTRUCTION; INSTRUMENT;
AIRBORNE; STANDS; LASER; PHOTOSYNTHESIS; ECHIDNA(R); TRANSFORM
AB Understanding canopy radiation regimes is critical to successfully modeling vegetation growth and function. For instance, the vertical distribution of photosynthetically active radiation (PAR) affects vegetation growth, informative upon carbon and energy cycling. Availing upon advances in information capture and computing power, geometrically explicit modeling of forest structure becomes increasingly possible: A primary challenge however is acquiring the forest mensuration data required to parameterize these models and the related automation of modeling forest structure. In this research, to address these issues we employ a novel and automated approach that capitalizes upon the rich information afforded by ground-based laser scanning technology. The method is implemented in two steps: in the first step, geometric explicit models of canopy structure are created from the ground-based laser scanning data. These geometric explicit models are used to simulate the vertical range to first hit. In the second step, we derive canopy gap probability from full waveform laser scanning data which have been used in a number of studies for characterization of radiation transmission Uupp et al., 2009; Yang et al., 2010) and do not require any geometric explicit modeling. The radiative consistency of the geometric explicit models from step 1 is validated against the gap probabilities of step 2. The results show a strong relationship between the radiative transmission properties of the geometric models and canopy gap probabilities at plot level (R = 0.91 to 0.97), while the geometric models suggest the additional benefit to serve as a bridge in scaling between shoot level and canopy level radiation. (C) 2013 Elsevier Inc. All rights reserved.
C1 [van Leeuwen, Martin; Coops, Nicholas C.] Univ British Columbia, Vancouver, BC V6T 1Z4, Canada.
[Hilker, Thomas] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Hilker, Thomas] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA.
[Wulder, Michael A.] Nat Resources Canada, Canadian Forest Serv, Victoria, BC V8Z 1M5, Canada.
[Newnham, Glenn J.; Culvenor, Darius S.] CSIRO, Clayton, Vic 3139, Australia.
RP van Leeuwen, M (reprint author), Univ British Columbia, 2424 Main Mall, Vancouver, BC V6T 1Z4, Canada.
EM vanleeuwen.martin@gmail.com
RI van Leeuwen, Martin/B-3947-2013; Coops, Nicholas/J-1543-2012; Newnham,
Glenn/G-8115-2011; Wulder, Michael/J-5597-2016
OI van Leeuwen, Martin/0000-0003-2572-2088; Coops,
Nicholas/0000-0002-0151-9037; Wulder, Michael/0000-0002-6942-1896
FU NSERC; Government of Canada through the Lodgepole Pine Partnership
Project; Canadian Forest Service; Canadian Wood Fibre Centre
FX We would like to express our thanks to members of the Integrated Remote
Sensing Studio, members of the Biometerology and Soil Physics Group, Dr.
Andrew Black and Zoran Nesic, University of British Columbia for their
assistance with the field work, and four anonymous reviewers for their
constructive feedback as well as Dr. Widlowski for advice regarding ray
tracer validation. Parts of this research are funded by an NSERC
Discovery grant to Dr. Coops. Additional funding was received from the
Government of Canada through the Lodgepole Pine Partnership Project
funded by the Canadian Forest Service and the Canadian Wood Fibre
Centre.
NR 66
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Z9 15
U1 0
U2 56
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2013
VL 136
BP 286
EP 300
DI 10.1016/j.rse.2013.04.019
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 186PC
UT WOS:000322055600025
ER
PT J
AU Zhao, F
Yang, XY
Strahler, AH
Schaaf, CL
Yao, T
Wang, ZS
Roman, MO
Woodcock, CE
Ni-Meister, W
Jupp, DLB
Lovell, JL
Culvenor, DS
Newnham, GJ
Tang, H
Dubayah, RO
AF Zhao, Feng
Yang, Xiaoyuan
Strahler, Alan H.
Schaaf, Crystal L.
Yao, Tian
Wang, Zhuosen
Roman, Miguel O.
Woodcock, Curtis E.
Ni-Meister, Wenge
Jupp, David L. B.
Lovell, Jenny L.
Culvenor, Darius S.
Newnham, Glenn J.
Tang, Hao
Dubayah, Ralph O.
TI A comparison of foliage profiles in the Sierra National Forest obtained
with a full-waveform under-canopy EVI lidar system with the foliage
profiles obtained with an airborne full-waveform LVIS lidar system
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Foliage profile; Ground-based full-waveform lidar; Airborne
full-waveform lidar system; EVI; LVIS
ID GROUND-BASED LIDAR; LEAF-AREA INDEX; VEGETATION STRUCTURE; INDIVIDUAL
TREES; LASER ALTIMETER; LAI PROFILES; BIOMASS; STANDS; VALIDATION;
TOPOGRAPHY
AB Foliage profiles retrieved from a scanning, terrestrial, near-infrared (1064 nm), full-waveform lidar, the Echidna Validation Instrument (EVI), agree well with those obtained from an airborne, near-infrared, full-waveform, large footprint lidar, the Lidar Vegetation Imaging Sensor (LVIS). We conducted trials at 5 plots within a conifer stand at Sierra National Forest in August, 2008. Foliage profiles retrieved from these two lidar systems are closely correlated (e.g., r = 0.987 at 100 m horizontal distances) at large spatial coverage while they differ significantly at small spatial coverage, indicating the apparent scanning perspective effect on foliage profile retrievals. Also we noted the obvious effects of local topography on foliage profile retrievals, particularly on the topmost height retrievals. With a fine spatial resolution and a small beam size, terrestrial lidar systems complement the strengths of the airborne lidars by making a detailed characterization of the crowns from a small field site, and thereby serving as a validation tool and providing localized tuning information for future airborne and spaceborne lidar missions. Published by Elsevier Inc.
C1 [Zhao, Feng; Yang, Xiaoyuan; Strahler, Alan H.; Schaaf, Crystal L.; Yao, Tian; Wang, Zhuosen; Woodcock, Curtis E.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Zhao, Feng; Tang, Hao; Dubayah, Ralph O.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Yang, Xiaoyuan; Schaaf, Crystal L.; Wang, Zhuosen] Univ Massachusetts, Boston, MA 02125 USA.
[Roman, Miguel O.] NASA Goddard Space Flight Ctr, Terr Informat Syst Lab Code 619, Greenbelt, MD 20705 USA.
[Ni-Meister, Wenge] CUNY Hunter Coll, Dept Geog, New York, NY 10065 USA.
[Jupp, David L. B.] CSIRO Marine & Atmospher Res, Canberra, ACT 2601, Australia.
[Lovell, Jenny L.] CSIRO Marine & Atmospher Res, Hobart, Tas 7000, Australia.
[Culvenor, Darius S.] Environm Sensing Syst, Melbourne, Vic, Australia.
[Newnham, Glenn J.] CSIRO Land & Water, Clayton, Vic 3169, Australia.
RP Zhao, F (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
EM fengbjfu@gmail.com
RI Beckley, Matthew/D-4547-2013; Newnham, Glenn/G-8115-2011; Tang,
Hua/K-4948-2016;
OI Tang, Hua/0000-0002-6685-6165; Jupp, David/0000-0002-9467-1344
FU NASA [NNG06GI92G, NNX08AE94A]; NSF [MRI-0923389]
FX This research was supported by NASA under grants NNG06GI92G and
NNX08AE94A and NSF under grant MRI-0923389. The authors gratefully
acknowledge the assistance of Mitchell Schull, Pontus Olofsson, Mary
LeeAnn King, Sage Sheldon, Amanda Sharon Whitehurst, Anupam Anand and
Anuradha Swatantran at Sierra National Forest sites. We are also
grateful to the many suggestions made by reviewers that significantly
improved our paper.
NR 29
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U1 5
U2 62
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2013
VL 136
BP 330
EP 341
DI 10.1016/j.rse.2013.05.020
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 186PC
UT WOS:000322055600028
ER
PT J
AU Musselman, KN
Margulis, SA
Molotch, NP
AF Musselman, Keith N.
Margulis, Steven A.
Molotch, Noah P.
TI Estimation of solar direct beam transmittance of conifer canopies from
airborne LiDAR
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Forest canopy; LiDAR; Voxel model; Ray-tracing; Solar direct beam
radiation
ID LASER SCANNER DATA; LEAF-AREA INDEX; FOREST CANOPIES; GAP FRACTION;
SHORTWAVE IRRADIANCE; LIGHT TRANSMITTANCE; STREAM TEMPERATURE; SNOW
COVER; RADIATION; ENERGY
AB The utility of airborne scanning LiDAR data to estimate solar direct beam canopy transmittance in complex, forested terrain was evaluated. Twenty-four hemispherical photos were used to produce ground-based estimates of solar direct beam canopy transmittance. The photo estimates were used to develop and evaluate two spatially distributed canopy transmittance models: 1) a Beer's Law-type transmittance model based on LiDAR-derived canopy metrics, and 2) a solar raytrace model applied to a three-dimensional canopy model. The models were used to estimate solar direct beam canopy transmittance at five-minute resolution for all days between the winter and summer solstices over an 800 m by 700 m domain at 1 m horizontal grid spacing. When compared to estimates from hemispherical photos, the raytrace model resolved the complex seasonal and diurnal variability of solar direct beam canopy transmittance resulting from individual trees and localized canopy structure. The Beer's-type model was unable to resolve these detailed factors. The two models exhibited similar and relatively low normalized daily mean error values from December to early March. Later in the season (01 March-21 June), the model differences were pronounced; the daily mean and standard deviation of the error values for the Beer's-type and raytrace models were 13% +/- 10% and 8% +/- 6%, respectively. The results confirm previously known limitations of Beer's Law when used to estimate sub-canopy solar beam irradiance under heterogeneous canopy conditions. Averaged over the spatial domain, the Beer's-type model estimated 21% and 48% lower canopy transmittance than the raytrace model on 01 March and 03 May, respectively. The Beer's-type model was unable to represent the seasonal increase in areal average canopy transmission contributed from small canopy gaps. Finally, both distributed models were used to simulate the cumulative solar beam irradiance during the 2010 snowmelt season. The raytrace model was shown to capture a high level of variability necessary to simulate explicit stand-scale solar irradiance that strongly influences spatiotemporal patterns of snowmelt, soil water availability, and the partition and exchange of energy within heterogeneous forest ecosystems. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Musselman, Keith N.; Margulis, Steven A.] Univ Calif Los Angeles, Dept Civil & Environm Engn, Los Angeles, CA 90095 USA.
[Musselman, Keith N.; Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Musselman, Keith N.; Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Musselman, KN (reprint author), Univ Saskatchewan, Ctr Hydrol, 117 Sci Pl, Saskatoon, SK S7N 5C8, Canada.
EM keith.musselman@usask.ca
RI Molotch, Noah/C-8576-2009
FU National Science Foundation [EAR-071160, EAR-1032295, EAR-1032308,
EAR-1141764]; Southern Sierra Critical Zone Observatory [EAR-0725097];
Mountain Research Initiative, NASA [NNX11AK35G]; NASA Earth System
Science Fellowship; [EAR-0619947]
FX Funding for this work was provided in part by National Science
Foundation grants EAR-071160, EAR-1032295, EAR-1032308, EAR-1141764, the
Southern Sierra Critical Zone Observatory (EAR-0725097), a Major
Research Instrumentation grant (EAR-0619947), the Mountain Research
Initiative, NASA grant NNX11AK35G and a NASA Earth System Science
Fellowship. The authors thank J. Pomeroy for his constructive feedback
on an early version of the manuscript, P. Kirchner and R. Bales for
field support, and three anonymous reviewers for valuable input that
greatly improved the paper.
NR 64
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Z9 22
U1 2
U2 48
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 SEP
PY 2013
VL 136
BP 402
EP 415
DI 10.1016/j.rse.2013.05.021
PG 14
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 186PC
UT WOS:000322055600033
ER
PT J
AU Small, C
Milesi, C
AF Small, Christopher
Milesi, Cristina
TI Multi-scale standardized spectral mixture models
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Spectral mixture model; Landsat; World View-2; Scale; Vegetation index
ID VEGETATION COVER; COEFFICIENTS; REFLECTANCE; VALIDATION; ABUNDANCE;
INDEXES
AB Linear spectral mixture models can be standardized by using endmembers that span the global mixing space. By combining the benefits of location-specific mixture models with standardized spectral indices, standardized mixture models offer consistency, simplicity, inclusivity and applicability. We construct a globally representative mixing space using a spectrally diverse collection of 100 Landsat ETM+ (Thematic Mapper 8: Enhanced Thematic Mapper+) subscenes. Global composites of 100,000,000 Landsat spectra, constructed from both exoatmospheric reflectance and atmospherically corrected surface reflectance, represent the spectral diversity of a wide range of terrestrial environments. Principal Component (PC) Analysis of the global composite shows that 99% of the spectral variance can be represented in a 3-dimensional mixing space of the low order PCs. Within this 3D space 98% of spectra are contained within a tetrahedral hull bounded by a continuous plane of substrates, and well-defined apexes corresponding to vegetation and dark endmembers. Suites of individual substrate, vegetation and dark endmember spectra are used to derive mean endmembers and to quantify the effects of endmember variability on fractions estimated from a standardized Substrate, Vegetation, and Dark (SVD) linear mixture model. Maximum endmember variability introduces less than 0.05 difference in S, V, and D fractions for most SVD models constructed from individual pixel endmember spectra giving less than 0.05 model misfit for more than 97% of pixels in the global composite. The mean SVD endmembers define a standard global mixture model for Landsat spectra. These SVD endmembers can be used to model mixed reflectance spectra from other sensors with similar spectral responses to Landsat ETM+. Comparisons of endmember fractions estimated from coincident acquisitions of Landsat TM and ETM + and WorldView-2 imagery show strong linear scaling for vegetation and dark fractions. Substrate fractions do not scale as linearly for the urban validation sites because the Landsat substrate endmember does not accurately represent the impervious surfaces imaged by World View-2. Comparisons of Landsat and WorldView-2 unmixed with the same Visible-Near Infrared (VNIR) endmembers derived from the global Landsat endmembers are also strongly correlated but with reduced bias. This linear scaling suggests that the Landsat global endmembers may provide a basis for standardized mixture models for WorldView-2 and other broadband sensors with spectral response similar to Landsat TM and ETM+. Comparisons of vegetation fractions with vegetation indices for the global composite show strong linear correspondence for Tasseled Cap Greenness and Enhanced Vegetation Index, with some degree of saturation at high fractions for the Soil Adjusted Vegetation Index and a wide range of responses for the Normalized Difference Vegetation Index. (C) 2013 Published by Elsevier Inc.
C1 [Small, Christopher] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Milesi, Cristina] Calif State Univ Monterey Bay, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Small, C (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
EM csmall@columbia.edu
FU NASA Land-Cover and Land-Use Change (LCLUC) Program [NNA07CN16A]
FX This study was made possible through funding from the NASA Land-Cover
and Land-Use Change (LCLUC) Program (grant NNA07CN16A). We acknowledge
the use of the NASA Earth Exchange (NEX) for the processing of the
Landsat data. We thank the anonymous reviewers for the numerous helpful
comments and suggestions.
NR 26
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U1 1
U2 58
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2013
VL 136
BP 442
EP 454
DI 10.1016/j.rse.2013.05.024
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 186PC
UT WOS:000322055600036
ER
PT J
AU Tan, B
Masek, JG
Wolfe, R
Gao, F
Huang, CQ
Vermote, EF
Sexton, JO
Ederer, G
AF Tan, Bin
Masek, Jeffrey G.
Wolfe, Robert
Gao, Feng
Huang, Chengquan
Vermote, Eric F.
Sexton, Joseph O.
Ederer, Greg
TI Improved forest change detection with terrain illumination corrected
Landsat images
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Illumination correction; Topographic effect; Landsat; LEDAPS; TDA-SVM
ID SUPPORT VECTOR MACHINES; SURFACE REFLECTANCE; TM DATA; CLASSIFICATION;
DISTURBANCE
AB An illumination correction algorithm has been developed to improve the accuracy of forest change detection from Landsat-derived reflectance data. This algorithm is based on an empirical rotation model and was tested on Landsat image pairs over the Cherokee National Forest, Tennessee; Uinta-Wasatch-Cache National Forest, Utah; San Juan National Forest, Colorado; and Sinkyone Wilderness State Park, California. The illumination correction process successfully eliminated correlation between Landsat reflectance and illumination condition. Comparison to forest-change maps derived from uncorrected images showed significant disagreement, ranging from 23% to 45%. Validated against high-resolution (1 m or less) time-serial images, the illumination correction decreased overestimation of forest gains and losses and improved specificity in detection of major forest changes. The overall accuracy increases 34% at the Cherokee Forest site and about 10% at the other three sites. The disagreement rate between change maps from the original and corrected Landsat images increased with increasing terrain inclination angle, with the relationship between illumination condition and the disagreement rate following a V-shaped curve that varied among sites. The lowest disagreement rate occurred when illumination condition was slightly smaller than that of a horizontal field. The correction for topographic illumination should be considered as a standard pre-processing step for land cover classification and land use change detection, especially for mountainous areas. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Tan, Bin] Earth Resources Technol Inc, Laurel, MD 20707 USA.
[Tan, Bin; Masek, Jeffrey G.; Wolfe, Robert; Ederer, Greg] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gao, Feng] ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Huang, Chengquan; Vermote, Eric F.; Sexton, Joseph O.] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Sexton, Joseph O.] Sigma Space Corp, Lanham, MD 20706 USA.
[Ederer, Greg] Univ Maryland, Global Land Cover Facil, College Pk, MD 20742 USA.
RP Tan, B (reprint author), NASA, GSFC, Code 619, Laurel, MD 20707 USA.
EM bin.tan@nasa.gov
RI Wolfe, Robert/E-1485-2012; Masek, Jeffrey/D-7673-2012;
OI Wolfe, Robert/0000-0002-0915-1855; Huang, Chengquan/0000-0003-0055-9798
FU NASA Terrestrial Ecology Program; NASA MEASURES Program
FX Support for this research was provided by the NASA Terrestrial Ecology
Program and the NASA MEASURES Program. Thanks for three reviewers'
useful and constructive comments. USDA is an equal opportunity provider
and employer.
NR 31
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U1 2
U2 62
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP
PY 2013
VL 136
BP 469
EP 483
DI 10.1016/j.rse.2013.05.013
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 186PC
UT WOS:000322055600038
ER
PT J
AU Angal, A
Xiong, XX
Choi, T
Chander, G
Mishra, N
Helder, DL
AF Angal, Amit
Xiong, Xiaoxiong (Jack)
Choi, Taeyoung (Jason)
Chander, Gyanesh
Mishra, Nischal
Helder, Dennis L.
TI Impact of Terra MODIS Collection 6 on long-term trending comparisons
with Landsat 7 ETM+ reflective solar bands
SO REMOTE SENSING LETTERS
LA English
DT Article
ID DESERT SITES; CALIBRATION; PERFORMANCE
AB Recently, the Moderate Resolution Imaging Spectroradiometer (MODIS) Characterization Support Team (MCST) has worked closely with the science team members to make significant improvements in both Terra and Aqua MODIS sensors. These refinements are included in the newly released Collection 6 (C6) Level 1B (L1B) products, and they primarily mitigate the long-term drifts observed in the short-wavelength bands of the MODIS sensors. This letter focuses particularly on evaluating the improvement in the long-term on-orbit radiometric calibration stability of the Terra MODIS sensor by comparing the trends with the Landsat 7 (L7) Enhanced Thematic Mapper Plus (ETM+) sensor. In this study, Terra MODIS L1B products from both Collection 5 (C5) and C6 were used to compare the long-term top-of-atmosphere (TOA) reflectance trending of the Terra MODIS reflective solar bands (RSB) with spectrally matching bands of the L7 ETM+ sensors over the Committee on Earth Observation Satellites (CEOS) reference pseudo-invariant calibration sites (PICS). In addition, intensive statistical tests were performed to support the assessment of the observed long-term drifts. The results from the newly processed Terra MODIS C6 L1B products clearly show the excellent calibration stability (long-term drift within 2%) of the MODIS sensor with the multi-year drifts within the specified calibration uncertainty.
C1 [Angal, Amit] SSAI, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong (Jack)] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Choi, Taeyoung (Jason)] Sigma Space Corp, Lanham, MD 20706 USA.
[Chander, Gyanesh] US Geol Survey, Earth Resources Observat & Sci EROS Ctr, SGT Inc, Sioux Falls, SD 57198 USA.
[Mishra, Nischal; Helder, Dennis L.] S Dakota State Univ, Brookings, SD 57007 USA.
RP Angal, A (reprint author), SSAI, Lanham, MD 20706 USA.
EM amit.angal@ssaihq.com
RI Richards, Amber/K-8203-2015; Choi, Taeyoung/E-4437-2016
OI Choi, Taeyoung/0000-0002-4596-989X
FU US Geological Survey [G10PC00044]
FX The authors would like to thank the members of MCST for technical
interaction. Work at SGT, Inc. was performed under US Geological Survey
contract G10PC00044. Any use of trade, product or firm names is for
descriptive purposes only and does not imply endorsement by the US
Government.
NR 10
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U1 3
U2 17
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 2150-704X
J9 REMOTE SENS LETT
JI Remote Sens. Lett.
PD SEP 1
PY 2013
VL 4
IS 9
BP 873
EP 881
DI 10.1080/2150704X.2013.809496
PG 9
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA 183JY
UT WOS:000321812200005
ER
PT J
AU Yeomans, DK
Chamberlin, AB
AF Yeomans, Donald K.
Chamberlin, Alan B.
TI Comparing the Earth impact flux from comets and near-Earth asteroids
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Comets; Asteroids; Near-Earth objects; Earth impact rates
ID PERIOD COMETS
AB When compared to the discovered set of near-Earth asteroids, the Earth impact flux of all known active comets, including Jupiter family comets, Halley-type and long period comets, is below 1%. However, the comet impact fluxes may be higher for those objects large enough to cause extinction level events. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Yeomans, Donald K.; Chamberlin, Alan B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yeomans, DK (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Donald.k.yeomans@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX A portion of this research represents an update and extension of work
carried out by the first author [17]. 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 17
TC 4
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U1 1
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP
PY 2013
VL 90
IS 1
SI SI
BP 3
EP 5
DI 10.1016/j.actaastro.2012.03.006
PG 3
WC Engineering, Aerospace
SC Engineering
GA 182EE
UT WOS:000321723700002
ER
PT J
AU Foster, C
Bellerose, J
Mauro, D
Jaroux, B
AF Foster, Cyrus
Bellerose, Julie
Mauro, David
Jaroux, Belgacem
TI Mission concepts and operations for asteroid mitigation involving
multiple gravity tractors
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Asteroid deflection; Gravity tractor; Multiple spacecraft
AB The gravity tractor concept is a proposed method to deflect an imminent asteroid impact through gravitational tugging over a time scale of years. In this study, we present mission scenarios and operational considerations for asteroid mitigation efforts involving multiple gravity tractors. We quantify the deflection performance improvement provided by a multiple gravity tractor campaign and assess its sensitivity to staggered launches. We next explore several proximity operation strategies to accommodate multiple gravity tractors at a single asteroid including formation-flying and mechanically-docked configurations. Finally, we utilize 99942 Apophis as an illustrative example to assess the performance of a multiple gravity tractor campaign. (C) 2012 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Foster, Cyrus; Bellerose, Julie; Mauro, David; Jaroux, Belgacem] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Foster, Cyrus; Mauro, David] Univ Space Res Assoc, Mountain View, CA 94043 USA.
[Bellerose, Julie] Carnegie Mellon Univ, Moffett Field, CA 94035 USA.
RP Foster, C (reprint author), NASA, Ames Res Ctr, M-S 202-3, Moffett Field, CA 94035 USA.
EM cyrus.foster@nasa.gov
FU NASA Ames Research Center; Ames Mission Design Center
FX The authors thank NASA Ames Research Center and the Ames Mission Design
Center for their support and feedback throughout this study.
NR 8
TC 2
Z9 2
U1 0
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP
PY 2013
VL 90
IS 1
SI SI
BP 112
EP 118
DI 10.1016/j.actaastro.2012.10.010
PG 7
WC Engineering, Aerospace
SC Engineering
GA 182EE
UT WOS:000321723700015
ER
PT J
AU Adamczyk, AM
Norbury, JW
Townsend, LW
AF Adamczyk, Anne M.
Norbury, John W.
Townsend, Lawrence W.
TI Weisskopf-Ewing and Hauser-Feshbach calculations of photonuclear cross
sections used for electromagnetic dissociation
SO RADIATION PHYSICS AND CHEMISTRY
LA English
DT Article
DE Photonuclear reactions; Weisskopf-Ewing; Hauser-Feshbach
ID MONTE-CARLO CALCULATIONS; NUCLEAR EVAPORATION
AB The Weisskopf-Ewing (WE) and Hauser-Feshbach (HF) theory are statistical methods, which are often used to calculate photonuclear cross sections for compound nucleus reactions. In our past work, WE methodology was presented and photonuclear reaction cross sections for nucleon emission were calculated using WE theory. Here, our previous results, which neglect pre-equilibrium emissions and do not include multiple particle emission, are compared to those calculated with HF theory and experimental data. For the reactions considered herein, it is found that the WE theory and HF method are in reasonable agreement below the two neutron separation energy assuming an energy dependent branching ratio for intermediate and heavy nuclei. In addition, qualitative confidence of WE theory for electromagnetic dissociation (EMD) cross section calculations was found. (c) 2013 Elsevier Ltd. All rights reserved.
C1 [Adamczyk, Anne M.; Townsend, Lawrence W.] Univ Tennessee, Knoxville, TN 37996 USA.
[Norbury, John W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Adamczyk, AM (reprint author), Univ Tennessee, 315 Pasqua Engn Bldg, Knoxville, TN 37996 USA.
EM aadamczy@utk.edu; John.W.Norbury@nasa.goy; ltownsen@utk.edu
NR 26
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0969-806X
J9 RADIAT PHYS CHEM
JI Radiat. Phys. Chem.
PD SEP
PY 2013
VL 90
BP 21
EP 25
DI 10.1016/j.radphyschem.2013.04.027
PG 5
WC Chemistry, Physical; Nuclear Science & Technology; Physics, Atomic,
Molecular & Chemical
SC Chemistry; Nuclear Science & Technology; Physics
GA 174SE
UT WOS:000321174900004
ER
PT J
AU Chambon, P
Roca, R
Jobard, I
Capderou, M
AF Chambon, Philippe
Roca, Remy
Jobard, Isabelle
Capderou, Michel
TI The Sensitivity of Tropical Rainfall Estimation From Satellite to the
Configuration of the Microwave Imager Constellation
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Constellation; Global Precipitation Measurement Mission (GPMM);
Megha-Tropiques; microwave; Observing System Simulation Experiment;
precipitation; satellite; tropics
ID COMBINED PASSIVE MICROWAVE; PRECIPITATION ANALYSIS; SAMPLING ERROR;
SPACE; TRMM; RETRIEVAL; AFRICA; SCALES; GSMAP
AB The availability of rainfall-related measurements from space has greatly increased from the late 1980s with the Defense Meteorological Satellite Program and the launch of the Tropical Rainfall Measuring Mission in 1997 to the forthcoming Global Precipitation Measurement (GPM) program (GPM mission) whose core satellite is to be launched in 2014. The rainfall observing systems have become a constellation enhancing the frequency of measurements all over the globe. In this letter, the Megha-Tropiques TAPEER-BRAIN level-4 rainfall product is considered to explore what impacts the configuration of a microwave imager constellation has on accumulated rainfall and associated sampling error estimates at one-degree/one-day resolution in the tropics. One of the main findings of this letter is that sun-synchronous satellites providing observations separated of time intervals close to rainfall autocorrelation periods result only in small improvements of TAPEER-BRAIN quantitative precipitation estimations (i.e., rain and error estimations). By comparison, it is shown that the GPM constellation of satellites, particularly with satellites on low-inclination "equatorial" orbits, has a high contribution to the improvements of rain and error estimates. The methodology developed in this letter could be also useful to explore the sensitivity of rainfall estimates at finer space and timescales.
C1 [Chambon, Philippe] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Roca, Remy] OMP LEGOS, F-31400 Toulouse, France.
[Jobard, Isabelle; Capderou, Michel] Ecole Polytech, Lab Meteorol Dynam IPSL, F-91128 Palaiseau, France.
RP Chambon, P (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM remy.roca@legos.obs-mip.fr
NR 22
TC 3
Z9 3
U1 1
U2 11
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD SEP
PY 2013
VL 10
IS 5
BP 996
EP 1000
DI 10.1109/LGRS.2012.2227668
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 172IA
UT WOS:000320993900006
ER
PT J
AU Thompson, DR
Mandrake, L
Green, RO
Chien, SA
AF Thompson, David R.
Mandrake, Lukas
Green, Robert O.
Chien, Steve A.
TI A Case Study of Spectral Signature Detection in Multimodal and
Outlier-Contaminated Scenes
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Clustering methods; filters; geoscience and remote sensing;
hyperspectral imaging; hyperspectral sensors; matched filters; pattern
clustering; pattern recognition; remote sensing; signal processing
ID IMAGING SPECTROSCOPY; MATCHED-FILTER; SPECTROMETERS; IMAGERY; AVIRIS;
EARTH
AB Mapping localized spectral features in complex scenes demands sensitive and robust detection algorithms. This letter investigates two aspects of large images that can harm matched filter (MF) detection performance. First, multimodal backgrounds may violate normality assumptions. Second, outlier features can trigger false detections due to large projections onto the target vector. We review two state-of-the-art methods designed to resolve these issues. The background clustering of Funk et al. models multimodal backgrounds, and the mixture-tuned (MT) MF of Boardman and Kruse addresses outliers. We demonstrate that combining the two methods has additional performance benefits. An MT cluster MF shows effective performance on simulated and airborne data sets. We demonstrate target detection scenarios that evidence multimodality, outliers, and their combination. These experiments explore the performance of the component algorithms and the practical circumstances that can favor a combined approach.
C1 [Thompson, David R.; Mandrake, Lukas; Green, Robert O.; Chien, Steve A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Thompson, DR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU Advanced Multimission Operating System; Multimission Ground Support
Services office
FX The authors would like to thank data, laboratory access, and assistance
of the AVIRIS team at the Jet Propulsion Laboratory. The methodology was
matured with support from a technology development Grant under the
Advanced Multimission Operating System and the Multimission Ground
Support Services office. The authors also thank the review panel for
their help and insight. Researchers interested in obtaining these data
should directly contact the authors.
NR 26
TC 2
Z9 2
U1 1
U2 25
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD SEP
PY 2013
VL 10
IS 5
BP 1021
EP 1025
DI 10.1109/LGRS.2012.2227932
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 172IA
UT WOS:000320993900011
ER
PT J
AU Kokhanovsky, AA
Painemal, D
Rozanov, VV
AF Kokhanovsky, Alexander A.
Painemal, D.
Rozanov, V. V.
TI The Intercomparison of Satellite-Derived and In Situ Profiles of Droplet
Effective Radii in Marine Stratocumulus Clouds
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Airborne measurements; cloud remote sensing; effective radius; liquid
water path (LWP); Moderate Resolution Imaging Spectroradiometer (MODIS)
ID VOCALS-REX; MODIS
AB It was found that the satellite spectral measurements can be used not only for the determination of cloud top effective radii but also for retrieving the effective radii vertical profile in some specific cases (e.g., for low marine stratocumulus clouds with negligible effects of horizontal variability). The inversion algorithm was applied to Moderate Resolution Imaging Spectroradiometer (MODIS) radiances (at the wavelengths of 0.865, 1.24, 1.6, and 2.1 mu m), and the results were validated against in situ airborne measurements of cloud vertical profiles of the effective radius. We found that the results were more reliable for the cases with large vertical gradients of droplet sizes. The new retrieval method, based on the optimal estimation approach, enabled a higher accuracy of the liquid water path estimate than that produced with the standard MODIS vertically homogeneous algorithm.
C1 [Kokhanovsky, Alexander A.; Rozanov, V. V.] Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany.
[Painemal, D.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Kokhanovsky, AA (reprint author), Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany.
EM lsr@iup.physik.uni-bremen.de
RI Kokhanovsky, Alexander/C-6234-2016
OI Kokhanovsky, Alexander/0000-0001-7370-1164
NR 24
TC 0
Z9 0
U1 1
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 SEP
PY 2013
VL 10
IS 5
BP 1147
EP 1151
DI 10.1109/LGRS.2012.2233710
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 172IA
UT WOS:000320993900037
ER
PT J
AU Melin, F
Zibordi, G
Holben, BN
AF Melin, Frederic
Zibordi, Giuseppe
Holben, Brent N.
TI Assessment of the Aerosol Products From the SeaWiFS and MODIS
Ocean-Color Missions
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Aerosol Robotic Network (AERONET); aerosol optical thickness;
Moderate-Resolution Spectroradiometer (MODIS); ocean color; Sea-viewing
Wide Field-of-View Sensor (SeaWiFS); uncertainty
ID OPTICAL-THICKNESS; SATELLITE; CALIBRATION; REFLECTANCE; VALIDATION;
RETRIEVAL; AERONET; DEPTH
AB The aerosol products derived from the ocean-color missions Sea-viewing Wide Field-of-View Sensor (SeaWiFS) and Moderate-Resolution Spectroradiometer (MODIS) Aqua and Terra are compared with field measurements from globally distributed Aerosol Robotic Network (AERONET) sites. Validation statistics are found consistent for the three missions. The median absolute relative difference between SeaWiFS and AERONET aerosol optical thickness tau(alpha) is approximately 20% at all bands while it is slightly higher for both MODIS products (between 20% and 28%). This is associated with a larger relative bias (median of relative differences between satellite and AERONET ta) on the order of + 15% for these missions. With respect to previous processing versions, a noticeable improvement is seen in the representation of the spectral dependence of ta. The bias found for the Angstrom exponent varies from -0.08 to + 0.13 for the three missions.
C1 [Melin, Frederic; Zibordi, Giuseppe] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy.
[Holben, Brent N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Melin, F (reprint author), Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy.
EM frederic.melin@jrc.ec.europa.eu; giuseppe.zibordi@jrc.ec.europa.eu;
brent.n.holben@nasa.gov
FU European Commission, FP7 Project MyOcean [218812]
FX This work was supported in part by the European Commission, FP7 Project
MyOcean (N. 218812).
NR 26
TC 7
Z9 7
U1 1
U2 17
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD SEP
PY 2013
VL 10
IS 5
BP 1185
EP 1189
DI 10.1109/LGRS.2012.2235408
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 172IA
UT WOS:000320993900045
ER
PT J
AU Larson, KM
Ray, RD
Nievinski, FG
Freymueller, JT
AF Larson, Kristine M.
Ray, Richard D.
Nievinski, Felipe G.
Freymueller, Jeffrey T.
TI The Accidental Tide Gauge: A GPS Reflection Case Study From Kachemak
Bay, Alaska
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE GPS; multipath; reflections; tide gauge
AB For the last decade, it has been known that reflected GPS signals observed with specialized instruments could be used to measure sea level. In this letter, data from an existing geodetic-quality GPS site near Kachemak Bay, Alaska, are analyzed for a one-year time period. Daily sea-level variations are more than 7 m. Tidal coefficients have been estimated and compared with coefficients estimated from records from a traditional tide gauge at Seldovia Harbor, similar to 30 km away. The GPS and Seldovia estimates of M-2 and S-2 coefficients agree to better than 2%; much of this residual can be attributed to true differences in the tide over 30 km as it propagates up Kachemak Bay. For daily mean sea levels the agreement is 2.3 cm. Because a standard geodetic GPS receiver/antenna is used, this GPS instrument can measure long-term sea-level changes in a stable terrestrial reference frame.
C1 [Larson, Kristine M.; Nievinski, Felipe G.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
[Ray, Richard D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Freymueller, Jeffrey T.] Univ Alaska, Fairbanks, AK 99775 USA.
RP Larson, KM (reprint author), Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
EM kristinem.larson@gmail.com; richard.ray@nasa.gov; fgnievinski@gmail.com;
jeff.freymueller@gi.alaska.edu
RI Ray, Richard/D-1034-2012; Geremia Nievinski, Felipe/G-4897-2013
OI Geremia Nievinski, Felipe/0000-0002-3325-1987
FU [AGS0935725]; [EAR0948957]
FX This work was supported in part by AGS0935725 and EAR0948957.
NR 16
TC 22
Z9 22
U1 1
U2 24
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD SEP
PY 2013
VL 10
IS 5
BP 1200
EP 1204
DI 10.1109/LGRS.2012.2236075
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 172IA
UT WOS:000320993900048
ER
PT J
AU Rogge, MD
Leckey, CAC
AF Rogge, Matthew D.
Leckey, Cara A. C.
TI Characterization of impact damage in composite laminates using guided
wavefield imaging and local wavenumber domain analysis
SO ULTRASONICS
LA English
DT Article
DE Ultrasonic wavefield imaging; Windowed Fourier transforms; Guided waves;
Nondestructive evaluation; Structural health monitoring
ID WAFER ACTIVE SENSORS; LAMB WAVES; PROPAGATION; SCATTERING; ARRAYS
AB Delaminations in composite laminates resulting from impact events may be accompanied by minimal indication of damage at the surface. As such, inspections are required to ensure defects are within allowable limits. Conventional ultrasonic scanning techniques have been shown to effectively characterize the size and depth of delaminations but require physical contact with the structure and considerable setup time. Alternatively, a non-contact scanning laser vibrometer may be used to measure guided wave propagation in the laminate structure generated by permanently bonded transducers. A local Fourier domain analysis method is presented for processing guided wavefield data to estimate spatially dependent wavenumber values, which can be used to determine delamination depth. The technique is applied to simulated wavefields and results are analyzed to determine limitations of the technique with regards to determining defect size and depth. Based on simulation results, guidelines for application of the technique are developed. Finally, experimental wavefield data is obtained in quasi-isotropic carbon fiber reinforced polymer (CFRP) laminates with impact damage. The recorded wavefields are analyzed and wavenumber is measured to an accuracy of up to 8.5% in the region of shallow delaminations. These results show the promise of local wavenumber domain analysis to characterize the depth of delamination damage in composite laminates. The technique can find application in automated vehicle health assurance systems with potential for high detection rates and greatly reduced operator effort and setup time. Published by Elsevier B.V.
C1 [Rogge, Matthew D.; Leckey, Cara A. C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Rogge, MD (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM matt.d.rogge@gmail.com
NR 35
TC 41
Z9 41
U1 9
U2 83
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0041-624X
J9 ULTRASONICS
JI Ultrasonics
PD SEP
PY 2013
VL 53
IS 7
BP 1217
EP 1226
DI 10.1016/j.ultras.2012.12.015
PG 10
WC Acoustics; Radiology, Nuclear Medicine & Medical Imaging
SC Acoustics; Radiology, Nuclear Medicine & Medical Imaging
GA 166ZD
UT WOS:000320598800002
PM 23602558
ER
PT J
AU Pasareanu, CS
Visser, W
Bushnell, D
Geldenhuys, J
Mehlitz, P
Rungta, N
AF Pasareanu, Corina S.
Visser, Willem
Bushnell, David
Geldenhuys, Jaco
Mehlitz, Peter
Rungta, Neha
TI Symbolic PathFinder: integrating symbolic execution with model checking
for Java bytecode analysis
SO AUTOMATED SOFTWARE ENGINEERING
LA English
DT Article
DE Symbolic execution; Model checking; Testing; Java
ID GENERATION; PROGRAMS; VERIFICATION; EFFICIENT; SYSTEMS; TOOL
AB Symbolic PathFinder (SPF) is a software analysis tool that combines symbolic execution with model checking for automated test case generation and error detection in Java bytecode programs. In SPF, programs are executed on symbolic inputs representing multiple concrete inputs and the values of program variables are represented by expressions over those symbolic inputs. Constraints over these expressions are generated from the analysis of different paths through the program. The constraints are solved with off-the-shelf solvers to determine path feasibility and to generate test inputs. Model checking is used to explore different symbolic program executions, to systematically handle aliasing in the input data structures, and to analyze the multithreading present in the code. SPF incorporates techniques for handling input data structures, strings, and native calls to external libraries, as well as for solving complex mathematical constraints. We describe the tool and its application at NASA, in academia, and in industry.
C1 [Pasareanu, Corina S.; Bushnell, David; Mehlitz, Peter; Rungta, Neha] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Visser, Willem; Geldenhuys, Jaco] Univ Stellenbosch, ZA-7600 Stellenbosch, South Africa.
RP Pasareanu, CS (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM corina.s.pasareanu@nasa.gov; wvisser@cs.sun.ac.za;
david.h.bushnell@nasa.gov; jaco@cs.sun.ac.za; peter.c.mehlitz@nasa.gov;
neha.s.rungta@nasa.gov
NR 74
TC 21
Z9 22
U1 0
U2 23
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0928-8910
EI 1573-7535
J9 AUTOMAT SOFTW ENG
JI Automat. Softw. Eng.
PD SEP
PY 2013
VL 20
IS 3
SI SI
BP 391
EP 425
DI 10.1007/s10515-013-0122-2
PG 35
WC Computer Science, Software Engineering
SC Computer Science
GA 155QP
UT WOS:000319763400004
ER
PT J
AU Seker, I
AF Seker, Ilgin
TI Are Planetary Tides on the Sun and the Birthplace of Sunspots Related?
SO SOLAR PHYSICS
LA English
DT Article
DE Sunspots; Solar activity; Planets; Tides
AB We study whether the birthplaces of sunspots (defined as the location of first appearance in the photosphere) are related to the planetary tides on the Sun. The heliocentric longitudes of newly emerging sunspots are statistically compared to the longitudes of tidal peaks caused by the tidal planets Mercury, Venus, Earth, and Jupiter. The longitude differences between new sunspots and tidal planets (and their conjugate locations) as well as the magnitudes of the vertical and horizontal tidal forces at the birthplace of new sunspots are calculated. The statistical distributions are compared with simulation results calculated using a random sunspot distribution. The results suggest that the birthplaces of sunspots (in the photosphere) are independent of the positions of tidal planets and the strength of tidal forces caused by them. However, since the sunspots actually originate near the tachocline (well below the photosphere) and it takes considerable time for the disturbances to reach photosphere, we hesitate to conclude that the formation of sunspots are not related to planetary positions.
C1 [Seker, Ilgin] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Seker, Ilgin] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Seker, I (reprint author), NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM ilgin.seker@nasa.gov
FU NASA [NNX10AL50A]
FX This research was supported by a NASA Grant (NNX10AL50A) to the Catholic
University of America. I thank N. Gopalswamy from NASA for his support
and my NASA summer intern C. Zheng for her contributions.
NR 12
TC 1
Z9 1
U1 1
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2013
VL 286
IS 2
BP 303
EP 314
DI 10.1007/s11207-013-0288-6
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 145IC
UT WOS:000319007700001
ER
PT J
AU Hathaway, DH
AF Hathaway, D. H.
TI A Curious History of Sunspot Penumbrae
SO SOLAR PHYSICS
LA English
DT Article
DE Active regions; structure; Sunspots; penumbra; Sunspots; statistics;
Sunspots; umbra
ID MAGNETIC-FIELD; UMBRAL AREAS; SUN-SPOTS; RATIO; CYCLE
AB Daily records of sunspot group areas compiled by the Royal Observatory, Greenwich, from May of 1874 through 1976 indicate a curious history for the penumbral areas of the smaller sunspot groups. On average, the ratio of penumbral area to umbral area in a sunspot group increases from 5 to 6 as the total sunspot group area increases from 100 to 2000 mu Hem (a mu Hem is 10(-6) the area of a solar hemisphere). This relationship does not vary substantially with sunspot group latitude or with the phase of the sunspot cycle. However, for the sunspot groups with total areas < 100 mu Hem, this ratio changes dramatically and systematically through this historical record. The ratio for these smallest sunspots is near 5.5 from 1874 to 1900. After a rapid rise to more than 7 in 1905, it drops smoothly to less than 3 by 1930 and then rises smoothly back to more than 7 in 1961. It then returns to near 5.5 from 1965 to 1976. The smooth variation from 1905 to 1961 shows no indication of any step-like changes that might be attributed to changes in equipment or personnel. The overall level of solar activity was increasing monotonically during this time period when the penumbra-to-umbra area ratio dropped to less than half its peak value and then returned. If this history can be confirmed by other observations (e.g. Mt. Wilson or Kodaikanal), it may impact our understanding of penumbra formation, our dynamo models, and our estimates of historical changes in the solar irradiance.
C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Hathaway, DH (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM david.hathaway@nasa.gov
FU NASA through through a grant from the Heliophysics Causes and
Consequences of the Minimum of Solar Cycle 23/24 Program
FX The author thanks Lisa Upton for reviewing the paper and NASA for its
support of this research through a grant from the Heliophysics Causes
and Consequences of the Minimum of Solar Cycle 23/24 Program to NASA
Marshall Space Flight Center. Comments by an anonymous referee led to
significant improvements in the paper. Most importantly, the author
thanks the American taxpayers for supporting scientific research in
general and this research in particular.
NR 19
TC 3
Z9 3
U1 0
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2013
VL 286
IS 2
BP 347
EP 356
DI 10.1007/s11207-013-0291-y
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 145IC
UT WOS:000319007700004
ER
PT J
AU Le Chat, G
Zaslavsky, A
Meyer-Vernet, N
Issautier, K
Belheouane, S
Pantellini, F
Maksimovic, M
Zouganelis, I
Bale, SD
Kasper, JC
AF Le Chat, G.
Zaslavsky, A.
Meyer-Vernet, N.
Issautier, K.
Belheouane, S.
Pantellini, F.
Maksimovic, M.
Zouganelis, I.
Bale, S. D.
Kasper, J. C.
TI Interplanetary Nanodust Detection by the Solar Terrestrial Relations
Observatory/WAVES Low Frequency Receiver
SO SOLAR PHYSICS
LA English
DT Article
DE Interplanetary dust; Nanodust; In situ dust detection; Radio antennas;
STEREO/WAVES
ID PLASMA-WAVE INSTRUMENT; DUST PARTICLES; RING PLANE; GRAIN IMPACTS; COMET
HALLEY; VOYAGER-2; VEGA-2; RADIO; NEPTUNE; URANUS
AB New measurements using radio and plasma-wave instruments in interplanetary space have shown that nanometer-scale dust, or nanodust, is a significant contributor to the total mass in interplanetary space. Better measurements of nanodust will allow us to determine where it comes from and the extent to which it interacts with the solar wind. When one of these nanodust grains impacts a spacecraft, it creates an expanding plasma cloud, which perturbs the photoelectron currents. This leads to a voltage pulse between the spacecraft body and the antenna. Nanodust has a high charge/mass ratio, and therefore can be accelerated by the interplanetary magnetic field to the speed of the solar wind: significantly faster than the Keplerian orbital speeds of heavier dust. The amplitude of the signal induced by a dust grain grows much more strongly with speed than with mass of the dust particle. As a result, nanodust can produce a strong signal despite its low mass. The WAVES instruments on the twin Solar TErrestrial RElations Observatory spacecraft have observed interplanetary nanodust particles since shortly after their launch in 2006. After describing a new and improved analysis of the last five years of STEREO/WAVES Low Frequency Receiver data, we present a statistical survey of the nanodust characteristics, namely the rise time of the pulse voltage and the flux of nanodust. We show that previous measurements and interplanetary dust models agree with this survey. The temporal variations of the nanodust flux are also discussed.
C1 [Le Chat, G.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
[Le Chat, G.; Kasper, J. C.] NASA, Lunar Sci Inst, Moffett Field, CA USA.
[Le Chat, G.; Zaslavsky, A.; Meyer-Vernet, N.; Issautier, K.; Belheouane, S.; Pantellini, F.; Maksimovic, M.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France.
[Zouganelis, I.] Univ Paris 06, LPP, Ecole Polytech, CNRS, F-94107 St Maur Des Fosses, France.
[Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Le Chat, G (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
EM glechat@head.cfa.harvard.edu
RI Bale, Stuart/E-7533-2011; Kasper, Justin/D-1152-2010
OI Bale, Stuart/0000-0002-1989-3596; Kasper, Justin/0000-0002-7077-930X
FU CNES; CNRS; NASA
FX We thank the team who designed and built the instrument. The S/WAVES
data used here are produced by an international consortium of the
Observatoire de Paris (France), the University of Minnesota (USA), the
University of California Berkeley (USA), and NASA Goddard Space Flight
Center (USA). The French contribution was funded by CNES and CNRS, and
the USA institutions were funded by NASA.
NR 28
TC 9
Z9 9
U1 1
U2 20
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2013
VL 286
IS 2
BP 549
EP 559
DI 10.1007/s11207-013-0268-x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 145IC
UT WOS:000319007700016
ER
PT J
AU McLaren, S
Worden, P
AF McLaren, Stephen
Worden, Pete
TI One minute with ... Pete Worden
SO NEW SCIENTIST
LA English
DT Editorial Material
C1 [Worden, Pete] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU REED BUSINESS INFORMATION LTD
PI SUTTON
PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND
SN 0262-4079
J9 NEW SCI
JI New Sci.
PD AUG 31
PY 2013
VL 219
IS 2932
BP 27
EP 27
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 211AP
UT WOS:000323876800015
ER
PT J
AU Kaynak, Y
Karaca, HE
Noebe, RD
Jawahir, IS
AF Kaynak, Y.
Karaca, H. E.
Noebe, R. D.
Jawahir, I. S.
TI Tool-wear analysis in cryogenic machining of NiTi shape memory alloys: A
comparison of tool-wear performance with dry and MQL machining
SO WEAR
LA English
DT Article
DE Cryogenic machining; NiTi shape memory alloys; Progressive tool-wear;
MQL
ID COATED GROOVED TOOLS; NICKEL-BASED ALLOYS; CERAMIC TOOLS; CUTTING TOOLS;
TI-6AL-4V ALLOY; TITANIUM-ALLOY; CARBIDE TOOLS; INCONEL 718;
TEMPERATURE; BASE
AB Extremely high tool-wear rate in machining of NiTi shape memory alloys (SMAs) is one of the major reasons for limiting the use of conventional machining processes on NiTi. The present study begins to address this issue by examining the effects of cryogenic cooling on tool-wear rate and progressive tool-wear by comparing the new findings from cryogenic machining with results obtained from minimum quantity lubrication (MQL) and dry machining conditions. Flank wear at the nose region, notch wear at the depth of cut boundary, and resulting machining performance criteria such as force components and surface quality of machined samples were studied. The findings from this research demonstrate that cryogenic cooling has a profound effect on controlling tool-wear rate and that the progressive tool-wear in machining of NiTi shape memory alloys can be significantly reduced by cryogenic machining. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Kaynak, Y.; Karaca, H. E.; Jawahir, I. S.] Univ Kentucky, Inst Sustainable Mfg, Lexington, KY 40506 USA.
[Kaynak, Y.] Univ Marmara, Mech & Machine Elements Div, TR-34722 Istanbul, Turkey.
[Noebe, R. D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
RP Kaynak, Y (reprint author), Univ Kentucky, Inst Sustainable Mfg, Lexington, KY 40506 USA.
EM yusuf_kaynak@yahoo.com
RI Jawahir, I.S./E-8447-2014
FU NASA FAP Aeronautical Sciences Project; NASA EPSCOR Program [NNX11AQ31A]
FX The authors sincerely thank Mr. Charles Arvin for his help with the
machining experiments and discussions with David Brinkman on machining
of NiTi. Support from the NASA FAP Aeronautical Sciences Project and the
NASA EPSCOR Program under Grant no. NNX11AQ31A is greatly acknowledged.
NR 63
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U1 4
U2 27
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0043-1648
J9 WEAR
JI Wear
PD AUG 30
PY 2013
VL 306
IS 1-2
BP 51
EP 63
DI 10.1016/j.wear.2013.05.011
PG 13
WC Engineering, Mechanical; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 276AU
UT WOS:000328721300008
ER
PT J
AU Autsavapromporn, N
Suzuki, M
Plante, I
Liu, CH
Uchihori, Y
Hei, TK
Azzam, EI
Murakami, T
AF Autsavapromporn, Narongchai
Suzuki, Masao
Plante, Ianik
Liu, Cuihua
Uchihori, Yukio
Hei, Tom K.
Azzam, Edouard I.
Murakami, Takeshi
TI Participation of gap junction communication in potentially lethal damage
repair and DNA damage in human fibroblasts exposed to low- or high-LET
radiation
SO MUTATION RESEARCH-GENETIC TOXICOLOGY AND ENVIRONMENTAL MUTAGENESIS
LA English
DT Article
DE Gap junction intercellular communication; Potentially lethal damage
repair; Linear energy transfer; Ionizing radiation; Heavy-ion beams
ID ION SPECIES DEPENDENCE; MONTE-CARLO-SIMULATION; IRRADIATED HUMAN-CELLS;
DOUBLE-STRAND BREAKS; TRACK STRUCTURE; INTERCELLULAR COMMUNICATION;
IONIZING-RADIATION; ALPHA-PARTICLES; INACTIVATION; CULTURES
AB Existing research has not fully explained how different types of ionizing radiation (IR) modulate the responses of cell populations or tissues. In our previous work, we showed that gap junction intercellular communication (GJIC) mediates the propagation of stressful effects among irradiated cells exposed to high linear energy transfer (LET) radiations, in which almost every cells is traversed by an IR track. In the present study, we conducted an in-depth study of the role of GJIC in modulating the repair of potentially lethal damage (PLDR) and micronuclei formation in cells exposed to low- or high-LET IR. Confluent human fibroblasts were exposed in the presence or absence of a gap junction inhibitor to 200 kV X rays (LET similar to 1.7 keV/mu m), carbon ions (LET similar to 76 keV/mu m), silicon ions (LET similar to 113 keV/mu m) or iron ions (LET similar to 400 keV/mu m) that resulted in isosurvival levels. The fibroblasts were incubated for various times at 37 degrees C. As expected, high-LET IR were more effective than were low-LET X rays at killing cells and damaging DNA shortly after irradiation. However, when cells were held in a confluent state for several hours, PLDR associated with a reduction in DNA damage, occurred only in cells exposed to X rays. Interestingly, inhibition of GJIC eliminated the enhancement of toxic effects, which resulted in an increase of cell survival and reduction in the level of micronucleus formation in cells exposed to high, but not in those exposed to low-LET IR. The experiment shows that gap-junction communication plays an important role in the propagation of stressful effects among irradiated cells exposed to high-LET IR while GJIC has only a minimal effect on PLDR and DNA damage following low-LET irradiation. Together, our results show that PLDR and induction of DNA damage clearly depend on gap-junction communication and radiation quality. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Autsavapromporn, Narongchai; Suzuki, Masao; Liu, Cuihua; Murakami, Takeshi] Natl Inst Radiol Sci, Res Ctr Charged Particle Therapy, Chiba 2638555, Japan.
[Plante, Ianik] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA.
[Uchihori, Yukio] Natl Inst Radiol Sci, Res Dev & Support Ctr, Radiat Measurement Res Sect, Chiba 2638555, Japan.
[Hei, Tom K.] Columbia Univ, Med Ctr, Coll Phys & Surg, Dept Radiat Oncol,Ctr Radiol Res, New York, NY 10032 USA.
[Azzam, Edouard I.] Univ Med & Dent New Jersey, New Jersey Med Sch, Ctr Canc, Dept Radiol, Newark, NJ 07103 USA.
RP Suzuki, M (reprint author), Natl Inst Radiol Sci, Res Ctr Charged Particle Therapy, Chiba 2638555, Japan.
EM m_suzuki@nirs.go.jp
FU NIRS-HIMAC; JSPS KAKENHI Grant [23-01513, 18310042, 24620014]; Quantum
Beam Technology Program from the Japan Science and Technology Agency;
National Institutes of Health [P01-CA 49062-21]
FX We highly thank the staff in HIMAC at NIRS for their excellent support.
This study was supported by the Research Project with Heavy Ions at
NIRS-HIMAC and in part by JSPS KAKENHI Grant Number 23-01513, 18310042,
24620014 and the Quantum Beam Technology Program from the Japan Science
and Technology Agency. The authors would like to acknowledge support
from the National Institutes of Health grant P01-CA 49062-21 to EIA and
TKH. The authors sincerely apologize to those whose work was not cited
due to space constraints.
NR 44
TC 4
Z9 5
U1 1
U2 11
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1383-5718
EI 1879-3592
J9 MUTAT RES-GEN TOX EN
JI Mutat. Res. Genet. Toxicol. Environ. Mutagen.
PD AUG 30
PY 2013
VL 756
IS 1-2
SI SI
BP 78
EP 85
DI 10.1016/j.mrgentox.2013.07.001
PG 8
WC Biotechnology & Applied Microbiology; Genetics & Heredity; Toxicology
SC Biotechnology & Applied Microbiology; Genetics & Heredity; Toxicology
GA 233WN
UT WOS:000325600300011
PM 23867854
ER
PT J
AU Liu, CH
Kawata, T
Furusawa, Y
Zhou, GM
Inoue, K
Fukada, J
Kota, R
George, K
Cucinotta, F
Okayasu, R
AF Liu, Cuihua
Kawata, Tetsuya
Furusawa, Yoshiya
Zhou, Guangming
Inoue, Kohei
Fukada, Junichi
Kota, Ryuichi
George, Kerry
Cucinotta, Francis
Okayasu, Ryuichi
TI Chromosome aberrations in normal human fibroblasts analyzed in G(0)/G(1)
and G(2)/M phases after exposure in G(0) to radiation with different
linear energy transfer (LET)
SO MUTATION RESEARCH-GENETIC TOXICOLOGY AND ENVIRONMENTAL MUTAGENESIS
LA English
DT Article
DE Chromosome aberration; Premature chromosome condensation (PCC);
Fluorescence in situ hybridization (FISH); High-LET radiation; Cell
cycle arrest
ID POTENTIALLY LETHAL DAMAGE; IN-SITU HYBRIDIZATION; DOUBLE-STRAND BREAKS;
CELL-CYCLE ARREST; HUMAN-LYMPHOCYTES; X-RAYS; EXCHANGE FORMATION;
TIME-COURSE; FE-IONS; C-IONS
AB We have studied the induction of chromosome aberrations in human fibroblasts exposed in G(0)/G(1) to X-rays or heavy ions to study the influence of G(1) cell cycle arrest. Confluent normal fibroblasts were exposed to X-rays or accelerated particles with different LET values and chromosome aberrations were investigated in the first G(0)/G(1) and G(2)//M phase. The particles used here were 490 MeV/nucleon Si, 500 MeV/nucleon Fe, and 200 MeV/nucleon Fe ions. Cells were subcultured 24 h after exposure and premature chromosome condensation (PCC) was performed by fusion-induced method for analysis of G(0)/G(1) cells, and chemically-induced method for analysis of G(2) and metaphase cells. Chromosome damage was assessed in chromosomes 1 and 3 using whole chromosome fluorescence in situ hybridization (FISH). Cell cycle was analyzed by flow cytometry at different incubation times following subculture. After irradiation with 2 Gy of high-LET particles, the yields of chromosome aberrations and fragments were significantly higher in G(0)/G(1) phase than in G(2)/M phase, whereas similar yields of damage were measured in both phases after exposure to X-rays. In contrast, the yield of misrepair, assessed by the number of color junctions, was similar in the G(0)/G(1) and G(2)/M phases after exposure to either X-rays or high-LET particles. The yields of chromosome aberrations, fragments, and color junctions in both the G(0)/G(1) and the G(2)/M phases, increased with LET up to 200 keV/mu m, then decreased for 440 key/mu m Fe particles. A good correlation was found between chromosome aberrations in both G(0)/G(1) and G(2)/M cells and survival fractions after 2 Gy of different LET radiations, although the slopes were steeper for the G(0)/G(1) cells. Flow cytometry analysis indicated that high-LET particles induce more non cycling G(0)/G(1) cells within 48 h of subculture than X-rays, suggesting that chromosome aberrations scored at the G(2)/M phase may not accurately describe the true radiation effect. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Liu, Cuihua; Furusawa, Yoshiya] Natl Inst Radiol Sci, Res Ctr Charged Particle Therapy, Chiba 2638555, Japan.
[Kawata, Tetsuya; Fukada, Junichi; Kota, Ryuichi] Keio Univ, Sch Med, Dept Radiol, Tokyo 1608582, Japan.
[Okayasu, Ryuichi] Natl Inst Radiol Sci, Int Open Lab, Chiba 2638555, Japan.
[Zhou, Guangming] Chinese Acad Sci, Inst Modern Phys, Dept Space Radiobiol, Lanzhou 730000, Peoples R China.
[Inoue, Kohei] Chiba Univ, Grad Sch Med, Dept Radiol, Chiba 2608670, Japan.
[George, Kerry] Wyle Sci, Technol & Engn Grp, Houston, TX 77058 USA.
[Cucinotta, Francis] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Kawata, T (reprint author), Keio Univ, Sch Med, Dept Radiol, Tokyo 1608582, Japan.
EM tkawata@rad.med.keio.ac.jp; rokayasu@nirs.go.jp
RI Okayasu, Ryuichi/F-2071-2013; Furusawa, Yoshiya/A-4487-2012
OI Okayasu, Ryuichi/0000-0001-5091-7210; Furusawa,
Yoshiya/0000-0003-4213-7331
FU NIRS-HIMAC; Japan Society for the Promotion of Science (JSPS) KAKENHI
[24591859, 24249067, 23591849]
FX The authors thank the staff of the HIMAC for their help with the
heavy-ion irradiation. The authors also thank Dr. M. Noguchi for
technical help in flow cytometry. This study was supported by a research
project with Heavy Ions at NIRS-HIMAC and in part by Japan Society for
the Promotion of Science (JSPS) KAKENHI grants 24591859, 24249067 and
23591849. The authors gratefully acknowledge Mr. Takuo Takihana for his
support and assistance during this study.
NR 33
TC 1
Z9 1
U1 0
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1383-5718
EI 1879-3592
J9 MUTAT RES-GEN TOX EN
JI Mutat. Res. Genet. Toxicol. Environ. Mutagen.
PD AUG 30
PY 2013
VL 756
IS 1-2
SI SI
BP 101
EP 107
DI 10.1016/j.mrgentox.2013.05.005
PG 7
WC Biotechnology & Applied Microbiology; Genetics & Heredity; Toxicology
SC Biotechnology & Applied Microbiology; Genetics & Heredity; Toxicology
GA 233WN
UT WOS:000325600300014
PM 23688614
ER
PT J
AU Wang, ML
Saha, J
Cucinotta, FA
AF Wang, Minli
Saha, Janapriya
Cucinotta, Francis A.
TI Smad7 foci are present in micronuclei induced by heavy particle
radiation
SO MUTATION RESEARCH-GENETIC TOXICOLOGY AND ENVIRONMENTAL MUTAGENESIS
LA English
DT Article
DE High LET radiation; DNA repair; Micronuclei; Smad7; TGF beta/Smad
pathway
ID GROWTH-FACTOR-BETA; EPITHELIAL-MESENCHYMAL TRANSITION; DOUBLE-STRAND
BREAKS; DNA-DAMAGE RESPONSE; FACTOR-KAPPA-B; TGF-BETA; INDUCED
APOPTOSIS; MOLECULAR-MECHANISMS; MEDIATES APOPTOSIS; IONIZING-RADIATION
AB DNA damage and reactive oxygen species (ROS) generated by ionizing radiation (IR) activate DNA damage response (DDR) and cytokine signaling pathways, including double strand break (DSB) repair and TGF beta/Smad signaling pathway. Proteins assembled at IR-induced DSB sites can be visualized as foci, including gamma H2AX, 53BP1, ATM and ATF2. Unrepaired DSBs are thought to be one origin of micronuclei (MN), an indicator of genotoxic stress and chromosomal instability. Studies have detected gamma H2AX in IR-induced MN, indicating the presence of DSB in MN. Previously we reported that TGF beta downstream proteins Smad7 and phospho-Smad2 (pSmad2) co-localized with DDR proteins following radiation. Here we studied the status of Smad7 and pSmad2 in MN post high linear energy transfer (LET) radiation in human normal and cancerous cells. We observed gamma H2AX foci in IR-induced MN, whereas 53BP1 and ATF2 were absent. Interestingly, Smad7 foci, but not pSmad2, were detectable in both spontaneous and IR-induced MN. We compared the effect of particle track structures on the yield of MN using 5.6 MeV/u boron (B) and 600 MeV/u iron (Fe) particles with similar LET (200 and 180 keV/mu m, respectively) in human fibroblasts. The frequency of MN induced by B was lower than that by Fe particles, albeit the proportion of Smad7-positive to Smad7-negative MN remained constant. An increased frequency of spontaneous MN, with slightly higher ratio of Smad7 or gamma H2AX positive, was found in human prostate cancer cells (PD) compared to normal cells. 24 h after 1 Gy of Fe particles exposure, the yield of MN increased, and the majority (similar to 70%) carried gamma H2AX and Smad7. Phospho-ATM (Ser1981) foci were found in both spontaneous and IR-induced MN in PC3 cells, displaying a much lower frequency compared to gamma H2AX and Smad7. Our data suggest a uniquesole of Smad7 in IR-induced MN formation, which may associate with DNA repair, apoptosis and genomic instability. (C) 2013 Published by Elsevier B.V.
C1 [Wang, Minli; Saha, Janapriya] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA.
[Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM francis.a.cucinotta@nasa.gov
FU NASA Space Radiation Program [NNJ12ZSA001N]; US Department of Energy
[DE-AI02-10ER64969]
FX This study was supported by NASA Space Radiation Program (#NNJ12ZSA001N)
to Dr. Minli Wang and US Department of Energy (DE-AI02-10ER64969) to Dr.
Francis. A. Cucinotta.
NR 45
TC 4
Z9 4
U1 0
U2 3
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1383-5718
EI 1879-3592
J9 MUTAT RES-GEN TOX EN
JI Mutat. Res. Genet. Toxicol. Environ. Mutagen.
PD AUG 30
PY 2013
VL 756
IS 1-2
SI SI
BP 108
EP 114
DI 10.1016/j.mrgentox.2013.04.011
PG 7
WC Biotechnology & Applied Microbiology; Genetics & Heredity; Toxicology
SC Biotechnology & Applied Microbiology; Genetics & Heredity; Toxicology
GA 233WN
UT WOS:000325600300015
PM 23643526
ER
PT J
AU George, K
Rhone, J
Beitman, A
Cucinotta, FA
AF George, K.
Rhone, J.
Beitman, A.
Cucinotta, F. A.
TI Cytogenetic damage in the blood lymphocytes of astronauts: Effects of
repeat long-duration space missions
SO MUTATION RESEARCH-GENETIC TOXICOLOGY AND ENVIRONMENTAL MUTAGENESIS
LA English
DT Article
DE Biodosimetry; FISH; Chromosome; PCC; High-LET radiation; Space radiation
ID SHIELDING EFFECTIVENESS; RADIATION; DOSIMETRY; EXPLORATION; EXPOSURE;
RISKS
AB Human missions onboard the International Space Station (ISS) are increasing in duration and several astronauts have now participated in second ISS increments. The radiation environment in space is very different from terrestrial radiation exposure and it is still unclear if space flight effects and radiation from repeat missions are simply additive, which potentially confounds the assessment of the cumulative risk of radiation exposure. It has been shown that single space missions of a few months or more on the ISS can induce measureable increases in the yield of chromosome damage in the blood lymphocytes of astronauts, and it appears that cytogenetic biodosimetry can be used reliably to estimate equivalent dose and radiation risk. We have now obtained direct in vivo measurements of chromosome damage in blood lymphocytes of five astronauts before and after their first and second long duration space flights. Chromosome damage was assessed by fluorescence in situ hybridization technique using three different chromosome painting probes. All astronauts showed an increase in total exchanges and translocations after both the first and second flight. Biological dose measured using either individual assessment or a population assessment supports an additive risk model. (C) 2013 The Authors. Published by Elsevier B.V. All rights reserved.
C1 [George, K.; Beitman, A.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA.
[Rhone, J.] Univ Houston, Houston, TX USA.
[Cucinotta, F. A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP George, K (reprint author), Wyle Sci Technol & Engn Grp, Mail Code Wyle HAC 37A,1290 Hercules Dr, Houston, TX 77058 USA.
EM kerry.a.george@nasa.gov
NR 17
TC 10
Z9 10
U1 0
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1383-5718
EI 1879-3592
J9 MUTAT RES-GEN TOX EN
JI Mutat. Res. Genet. Toxicol. Environ. Mutagen.
PD AUG 30
PY 2013
VL 756
IS 1-2
SI SI
BP 165
EP 169
DI 10.1016/j.mrgentox.2013.04.007
PG 5
WC Biotechnology & Applied Microbiology; Genetics & Heredity; Toxicology
SC Biotechnology & Applied Microbiology; Genetics & Heredity; Toxicology
GA 233WN
UT WOS:000325600300023
PM 23639573
ER
PT J
AU Xue, XW
Hong, Y
Limaye, AS
Gourley, JJ
Huffman, GJ
Khan, SI
Dorji, C
Chen, S
AF Xue, Xianwu
Hong, Yang
Limaye, Ashutosh S.
Gourley, Jonathan J.
Huffman, George J.
Khan, Sadiq Ibrahim
Dorji, Chhimi
Chen, Sheng
TI Statistical and hydrological evaluation of TRMM-based Multi-satellite
Precipitation Analysis over the Wangchu Basin of Bhutan: Are the latest
satellite precipitation products 3B42V7 ready for use in ungauged
basins?
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE CREST model; A-priori parameter estimation; Hydrologic modeling
evaluation; Precipitation estimation
ID MODEL EVALUATION; ANALYSIS TMPA; RAINFALL; EQUIFINALITY; UNCERTAINTY;
CLASSIFICATION; PREDICTION; RESOLUTION; NETWORK; SYSTEM
AB The objective of this study is to quantitatively evaluate the successive Tropical Rainfall Measuring Mission (TRMM) Multi-satellite Precipitation Analysis (TMPA) products and further to explore the improvements and error propagation of the latest 3B42V7 algorithm relative to its predecessor 3B42V6 using the Coupled Routing and Excess Storage (CREST) hydrologic model in the mountainous Wangchu Basin of Bhutan. First, the comparison to a decade-long (2001-2010) daily rain gauge dataset reveals that: (1) 3B42V7 generally improves upon 3B42V6's underestimation both for the whole basin (bias from -41.15% to -8.38%) and for a 0.25 x 0.25 grid cell with high-density gauges (bias from -40.25% to 0.04%), though with modest enhancement of correlation coefficients (CC) (from 0.36 to 0.40 for basin-wide and from 0.37 to 0.41 for grid); and (2) 3B42V7 also improves its occurrence frequency across the rain intensity spectrum. Using the CREST model that has been calibrated with rain gauge inputs, the 3B42V6-based simulation shows limited hydrologic prediction NSCE skill (0.23 in daily scale and 0.25 in monthly scale) while 3B42V7 performs fairly well (0.66 in daily scale and 0.77 in monthly scale), a comparable skill score with the gauge rainfall simulations. After recalibrating the model with the respective TMPA data, significant improvements are observed for 3B42V6 across all categories, but not as much enhancement for the already-well-performing 3B42V7 except for a reduction in bias (from -26.98% to -4.81%). In summary, the latest 3B42V7 algorithm reveals a significant upgrade from 3B42V6 both in precipitation accuracy (i.e., correcting the underestimation) thus improving its potential hydrological utility. Forcing the model with 3B42V7 rainfall yields comparable skill scores with in situ gauges even without recalibration of the hydrological model by the satellite precipitation, a compensating approach often used but not favored by the hydrology community, particularly in ungauged basins. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Xue, Xianwu; Hong, Yang; Khan, Sadiq Ibrahim; Chen, Sheng] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73072 USA.
[Xue, Xianwu; Hong, Yang] Natl Weather Ctr, Adv Radar Res Ctr, Norman, OK 73072 USA.
[Limaye, Ashutosh S.] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, ZP11, Huntsville, AL 35805 USA.
[Gourley, Jonathan J.] NOAA, Natl Severe Storms Lab, Norman, OK 73072 USA.
[Huffman, George J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dorji, Chhimi] Minist Econ Affairs, Dept Hydromet Serv, Thimphu, Bhutan.
RP Hong, Y (reprint author), Natl Weather Ctr, Atmospher Radar Res Ctr, Suite 3630,120 David L Boren Blvd, Norman, OK 73072 USA.
EM yanghong@ou.edu
RI Hong, Yang/D-5132-2009; Huffman, George/F-4494-2014; Gourley,
Jonathan/C-7929-2016; Xue, Xianwu/C-8006-2016
OI Hong, Yang/0000-0001-8720-242X; Huffman, George/0000-0003-3858-8308;
Gourley, Jonathan/0000-0001-7363-3755; Xue, Xianwu/0000-0002-2106-6370
FU NASA/Marshall Space Flight Center [NNM11AB34P, NNMi2428088Q]
FX The current study was supported by the NASA/Marshall Space Flight Center
Grants NNM11AB34P and NNMi2428088Q to the University of Oklahoma.
NR 39
TC 69
Z9 76
U1 5
U2 34
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-1694
J9 J HYDROL
JI J. Hydrol.
PD AUG 30
PY 2013
VL 499
BP 91
EP 99
DI 10.1016/j.jhydrol.2013.06.042
PG 9
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA 220RY
UT WOS:000324605800009
ER
PT J
AU Schnittman, JD
AF Schnittman, Jeremy D.
TI The Curious Behavior of the Milky Way's Central Black Hole
SO SCIENCE
LA English
DT Editorial Material
ID SAGITTARIUS-A-ASTERISK; GALACTIC-CENTER
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Schnittman, JD (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM jeremy.d.schnittman@nasa.gov
NR 10
TC 0
Z9 0
U1 0
U2 3
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 AUG 30
PY 2013
VL 341
IS 6149
BP 964
EP 965
DI 10.1126/science.1243115
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 208BZ
UT WOS:000323652300026
PM 23990547
ER
PT J
AU Reeves, GD
Spence, HE
Henderson, MG
Morley, SK
Friedel, RHW
Funsten, HO
Baker, DN
Kanekal, SG
Blake, JB
Fennell, JF
Claudepierre, SG
Thorne, RM
Turner, DL
Kletzing, CA
Kurth, WS
Larsen, BA
Niehof, JT
AF Reeves, G. D.
Spence, H. E.
Henderson, M. G.
Morley, S. K.
Friedel, R. H. W.
Funsten, H. O.
Baker, D. N.
Kanekal, S. G.
Blake, J. B.
Fennell, J. F.
Claudepierre, S. G.
Thorne, R. M.
Turner, D. L.
Kletzing, C. A.
Kurth, W. S.
Larsen, B. A.
Niehof, J. T.
TI Electron Acceleration in the Heart of the Van Allen Radiation Belts
SO SCIENCE
LA English
DT Article
ID 1997 MAGNETIC CLOUD; RELATIVISTIC ELECTRONS; GEOMAGNETIC STORMS; ULF;
ENERGIZATION; MAGNETOSPHERE; CHORUS; POWER
AB The Van Allen radiation belts contain ultrarelativistic electrons trapped in Earth's magnetic field. Since their discovery in 1958, a fundamental unanswered question has been how electrons can be accelerated to such high energies. Two classes of processes have been proposed: transport and acceleration of electrons from a source population located outside the radiation belts (radial acceleration) or acceleration of lower-energy electrons to relativistic energies in situ in the heart of the radiation belts (local acceleration). We report measurements from NASA's Van Allen Radiation Belt Storm Probes that clearly distinguish between the two types of acceleration. The observed radial profiles of phase space density are characteristic of local acceleration in the heart of the radiation belts and are inconsistent with a predominantly radial acceleration process.
C1 [Reeves, G. D.; Henderson, M. G.; Morley, S. K.; Friedel, R. H. W.; Funsten, H. O.; Larsen, B. A.; Niehof, J. T.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM 87545 USA.
[Spence, H. E.] Univ New Hampshire, Each Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Baker, D. N.] Univ Colorado, Lab Atmospher & Space Res, Boulder, CO 80309 USA.
[Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blake, J. B.; Fennell, J. F.; Claudepierre, S. G.] Aerosp Corp, El Segundo, CA 90245 USA.
[Thorne, R. M.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[Turner, D. L.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Kletzing, C. A.; Kurth, W. S.] Univ Iowa, Dept Phys, Iowa City, IA 52242 USA.
RP Reeves, GD (reprint author), Los Alamos Natl Lab, Space Sci & Applicat Grp, POB 1663, Los Alamos, NM 87545 USA.
EM reeves@lanl.gov
RI Morley, Steven/A-8321-2008; Turner, Drew/G-3224-2012; Friedel,
Reiner/D-1410-2012; Funsten, Herbert/A-5702-2015; Larsen,
Brian/A-7822-2011; Henderson, Michael/A-3948-2011;
OI Reeves, Geoffrey/0000-0002-7985-8098; Morley,
Steven/0000-0001-8520-0199; Friedel, Reiner/0000-0002-5228-0281;
Funsten, Herbert/0000-0002-6817-1039; Larsen, Brian/0000-0003-4515-0208;
Henderson, Michael/0000-0003-4975-9029; Spence,
Harlan/0000-0002-2526-2205; Kletzing, Craig/0000-0002-4136-3348; Kurth,
William/0000-0002-5471-6202
FU RBSP-Energetic Particle, Composition, and Thermal Plasma under NASA
[NAS5-01072]
FX This work was supported by RBSP-Energetic Particle, Composition, and
Thermal Plasma funding under NASA's Prime contract no. NAS5-01072. All
Van Allen Probes (RBSP) observations used in this study, along with
display and analysis software, are publicly available at the Web site
www.rbsp-ect.lanl.gov.
NR 31
TC 146
Z9 148
U1 3
U2 20
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 AUG 30
PY 2013
VL 341
IS 6149
BP 991
EP 994
DI 10.1126/science.1237743
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 208BZ
UT WOS:000323652300039
PM 23887876
ER
PT J
AU Dai, L
Takahashi, K
Wygant, JR
Chen, L
Bonnell, J
Cattell, CA
Thaller, S
Kletzing, C
Smith, CW
MacDowall, RJ
Baker, DN
Blake, JB
Fennell, J
Claudepierre, S
Funsten, HO
Reeves, GD
Spence, HE
AF Dai, Lei
Takahashi, Kazue
Wygant, John R.
Chen, Liu
Bonnell, John
Cattell, Cynthia A.
Thaller, Scott
Kletzing, Craig
Smith, Charles W.
MacDowall, Robert J.
Baker, Daniel N.
Blake, J. Bernard
Fennell, Joseph
Claudepierre, Seth
Funsten, Herbert O.
Reeves, Geoffrey D.
Spence, Harlan E.
TI Excitation of poloidal standing Alfven waves through drift resonance
wave-particle interaction
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE drift resonance; poloidal standing wave; ring current
ID FREQUENCY GEOMAGNETIC-PULSATIONS; RING-CURRENT; HYDROMAGNETIC-WAVES;
GIANT PULSATIONS; MAGNETOSPHERE; BEHAVIOR; PLASMA; MODES; FIELD; ZONE
AB Drift-resonance wave-particle interaction is a fundamental collisionless plasma process studied extensively in theory. Using cross-spectral analysis of electric field, magnetic field, and ion flux data from the Van Allen Probe (Radiation Belt Storm Probes) spacecraft, we present direct evidence identifying the generation of a fundamental mode standing poloidal wave through drift-resonance interactions in the inner magnetosphere. Intense azimuthal electric field (E) oscillations as large as 10mV/m are observed, associated with radial magnetic field (B-r) oscillations in the dawn-noon sector near but south of the magnetic equator at L approximate to 5. The observed wave period, E/B-r ratio and the 90 degrees phase lag between B-r and E are all consistent with fundamental mode standing Poloidal waves. Phase shifts between particle fluxes and wave electric fields clearly demonstrate a drift resonance with approximate to 90 keV ring current ions. The estimated earthward gradient of ion phase space density provides a free energy source for wave generation through the drift-resonance instability. A similar drift-resonance process should occur ubiquitously in collisionless plasma systems. One specific example is the fishbone instability in fusion plasma devices. In addition, our observations have important implications for the long-standing mysterious origin of Giant Pulsations.
C1 [Dai, Lei; Wygant, John R.; Cattell, Cynthia A.; Thaller, Scott] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55414 USA.
[Takahashi, Kazue] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Chen, Liu] Zhejiang Univ, Inst Fus Theory & Simulat, Hangzhou 310003, Zhejiang, Peoples R China.
[Chen, Liu] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA.
[Bonnell, John] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Kletzing, Craig] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Smith, Charles W.; Spence, Harlan E.] Univ New Hampshire, Dept Phys, Inst Earth Oceans & Space, Durham, NH 03824 USA.
[MacDowall, Robert J.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Baker, Daniel N.] Univ Colorado Boulder, Atmospher & Space Phys Lab, Boulder, CO USA.
[Blake, J. Bernard; Fennell, Joseph; Claudepierre, Seth] Aerosp Corp, Los Angeles, CA 90009 USA.
[Funsten, Herbert O.; Reeves, Geoffrey D.] Los Alamos Natl Lab, Los Alamos, NM USA.
RP Dai, L (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55414 USA.
EM dai@physics.umn.edu
RI chen, liu/I-2297-2013; Funsten, Herbert/A-5702-2015; Reeves,
Geoffrey/E-8101-2011;
OI Funsten, Herbert/0000-0002-6817-1039; Reeves,
Geoffrey/0000-0002-7985-8098; Cattell, Cynthia/0000-0002-3805-320X;
Kletzing, Craig/0000-0002-4136-3348; Spence, Harlan/0000-0002-2526-2205
FU APL; NASA [NNX10AK93G]
FX Work at UMN was supported by a contract from APL for the development of
RBSP/EFW. Work at JHUAPL was supported by NASA grant NNX10AK93G. L. D.
thanks Kris Kersten, Aaron Breneman, Jianbao Tao, and Peter Schroeder
for developing and testing analysis tools for EFW electric field data.
NR 33
TC 38
Z9 38
U1 2
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 AUG 28
PY 2013
VL 40
IS 16
BP 4127
EP 4132
DI 10.1002/grl.50800
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 219SI
UT WOS:000324529000001
ER
PT J
AU Wagstaff, KL
Thompson, DR
Abbey, W
Allwood, A
Bekker, DL
Cabrol, NA
Fuchs, T
Ortega, K
AF Wagstaff, K. L.
Thompson, D. R.
Abbey, W.
Allwood, A.
Bekker, D. L.
Cabrol, N. A.
Fuchs, T.
Ortega, K.
TI Smart, texture-sensitive instrument classification for in situ rock and
layer analysis
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE onboard analysis; classification
ID AUTONOMOUS SCIENCE; LANDING SITE; ROVER; MARS
AB Science missions have limited lifetimes, necessitating an efficient investigation of the field site. The efficiency of onboard cameras, critical for planning, is limited by the need to downlink images to Earth for every decision. Recent advances have enabled rovers to take follow-up actions without waiting hours or days for new instructions. We propose using built-in processing by the instrument itself for adaptive data collection, faster reconnaissance, and increased mission science yield. We have developed a machine learning pixel classifier that is sensitive to texture differences in surface materials, enabling more sophisticated onboard classification than was previously possible. This classifier can be implemented in a Field Programmable Gate Array (FPGA) for maximal efficiency and minimal impact on the rest of the system's functions. In this paper, we report on initial results from applying the texture-sensitive classifier to three example analysis tasks using data from the Mars Exploration Rovers.
C1 [Wagstaff, K. L.; Thompson, D. R.; Abbey, W.; Allwood, A.; Bekker, D. L.; Fuchs, T.; Ortega, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cabrol, N. A.] NASA, Ames Res Ctr, Div Space Sci, SETI Inst, Moffett Field, CA 94035 USA.
RP Wagstaff, KL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kiri.l.wagstaff@jpl.nasa.gov
FU NASA Astrobiology Science and Technology Instrument Development program
[NNH10ZDA001N-ASTID]; National Aeronautics and Space Administration
FX The TextureCam project is supported by the NASA Astrobiology Science and
Technology Instrument Development program (NNH10ZDA001N-ASTID). The Mars
Exploration Rover images used in this study were obtained from the
Planetary Data System (PDS). We thank Matt Golombek, Rebecca Castano,
Ben Bornstein, and many students who contributed the manual rock labels
used in our rock-finding study. This work was carried out at the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with the National Aeronautics and Space Administration.
Government sponsorship acknowledged.
NR 20
TC 5
Z9 5
U1 1
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 AUG 28
PY 2013
VL 40
IS 16
BP 4188
EP 4193
DI 10.1002/grl.50817
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 219SI
UT WOS:000324529000012
ER
PT J
AU Behrenfeld, MJ
Hu, YX
Hostetler, CA
Dall'Olmo, G
Rodier, SD
Hair, JW
Trepte, CR
AF Behrenfeld, Michael J.
Hu, Yongxiang
Hostetler, Chris A.
Dall'Olmo, Giorgio
Rodier, Sharon D.
Hair, John W.
Trepte, Charles R.
TI Space-based lidar measurements of global ocean carbon stocks
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ocean; carbon; phytoplankton; satellite; lidar; CALIOP
ID PARTICULATE ORGANIC-CARBON; VOLUME SCATTERING FUNCTION;
OPTICAL-PROPERTIES; CHLOROPHYLL CONCENTRATION; PHYTOPLANKTON PHYSIOLOGY;
BEAM ATTENUATION; MUELLER MATRIX; BACKSCATTERING; COLOR; DYNAMICS
AB Global ocean phytoplankton biomass (C-phyto) and total particulate organic carbon (POC) stocks have largely been characterized from space using passive ocean color measurements. A space-based light detection and ranging (lidar) system can provide valuable complementary observations for C-phyto and POC assessments, with benefits including day-night sampling, observations through absorbing aerosols and thin cloud layers, and capabilities for vertical profiling through the water column. Here we use measurements from the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) to quantify global C-phyto and POC from retrievals of subsurface particulate backscatter coefficients (b(bp)). CALIOP b(bp) data compare favorably with airborne, ship-based, and passive ocean data and yield global average mixed-layer standing stocks of 0.44 Pg C for C-phyto and 1.9 Pg for POC. CALIOP-based C-phyto and POC data exhibit global distributions and seasonal variations consistent with ocean plankton ecology. Our findings support the use of spaceborne lidar measurements for advancing understanding of global plankton systems.
C1 [Behrenfeld, Michael J.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA.
[Hu, Yongxiang; Hostetler, Chris A.; Rodier, Sharon D.; Hair, John W.; Trepte, Charles R.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Dall'Olmo, Giorgio] Plymouth Marine Lab, Plymouth, Devon, England.
RP Behrenfeld, MJ (reprint author), Oregon State Univ, Dept Bot & Plant Pathol, Cordley Hall 2082, Corvallis, OR 97331 USA.
EM mjb@science.oregonstate.edu
RI Hu, Yongxiang/K-4426-2012
FU NASA's Ocean Biology and Biogeochemistry Program;
Aerosols-Clouds-Ecosystems Science Working Group; CALIPSO mission; UK
Natural Environment Research Council; National Oceanography Centre,
Southampton
FX This research was supported by funding from NASA's Ocean Biology and
Biogeochemistry Program, the Aerosols-Clouds-Ecosystems Science Working
Group, and the CALIPSO mission. We thank Robert O'Malley for assistance
with data analysis, Toby Westberry for manuscript comments, and the
CALIPSO team for CALIOP data analysis support. This study is a
contribution to the international IMBER project, and ship-based
measurements were in part supported by the UK Natural Environment
Research Council National Capability funding to Plymouth Marine
Laboratory and the National Oceanography Centre, Southampton. This is
contribution number 234 of the AMT programme.
NR 41
TC 14
Z9 14
U1 5
U2 35
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 AUG 28
PY 2013
VL 40
IS 16
BP 4355
EP 4360
DI 10.1002/grl.50816
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 219SI
UT WOS:000324529000042
ER
PT J
AU Fasullo, JT
Boening, C
Landerer, FW
Nerem, RS
AF Fasullo, John T.
Boening, Carmen
Landerer, Felix W.
Nerem, R. Steven
TI Australia's unique influence on global sea level in 2010-2011
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE global sea level; water cycle; Australian climate; energy cycle; climate
variability
ID TIME-SERIES; TOPEX/POSEIDON; JASON-1; WATER
AB In 2011, a significant drop in global sea level occurred that was unprecedented in the altimeter era and concurrent with an exceptionally strong La Nina. This analysis examines multiple data sets in exploring the physical basis for the drop's exceptional intensity and persistence. Australia's hydrologic surface mass anomaly is shown to have been a dominant contributor to the 2011 global total, and associated precipitation anomalies were among the highest on record. The persistence of Australia's mass anomaly is attributed to the continent's unique surface hydrology, which includes expansive arheic and endorheic basins that impede runoff to ocean. Based on Australia's key role, attribution of sea level variability is addressed. The modulating influences of the Indian Ocean Dipole and Southern Annular Mode on La Nina teleconnections are found to be key drivers of anomalous precipitation in the continent's interior and the associated surface mass and sea level responses.
C1 [Fasullo, John T.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Boening, Carmen; Landerer, Felix W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Nerem, R. Steven] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA.
RP Fasullo, JT (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
EM fasullo@ucar.edu
OI Landerer, Felix/0000-0003-2678-095X
FU NASA [NNG06GB91G, NNH11ZDA001N]; NSF [NSF-AGS-1243107]; National Science
Foundation; National Aeronautics and Space Administration
FX John T. Fasullo's participation in this work is supported by NASA awards
NNG06GB91G and NNH11ZDA001N and NSF award NSF-AGS-1243107. The National
Center for Atmospheric Research (NCAR) is sponsored by the National
Science Foundation. 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.
NR 23
TC 53
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U1 2
U2 31
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 AUG 28
PY 2013
VL 40
IS 16
BP 4368
EP 4373
DI 10.1002/grl.50834
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 219SI
UT WOS:000324529000045
ER
PT J
AU Streets, DG
Shindell, DT
Lu, ZF
Faluvegi, G
AF Streets, David G.
Shindell, Drew T.
Lu, Zifeng
Faluvegi, Greg
TI Radiative forcing due to major aerosol emitting sectors in China and
India
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE radiative forcing; aerosols; China; India; radiative forcing; aerosols;
China; India
ID FUTURE CLIMATE SIMULATIONS; REGIONAL EMISSIONS; IMPACTS; HEALTH; OZONE
AB Understanding the radiative forcing caused by anthropogenic aerosol sources is essential for making effective emission control decisions to mitigate climate change. We examined the net direct plus indirect radiative forcing caused by carbonaceous aerosol and sulfur emissions in key sectors of China and India using the GISS-E2 chemistry-climate model. Diesel trucks and buses (67 mW m(-2)) and residential biofuel combustion (52 mW m(-2)) in India have the largest global mean, annual average forcings due mainly to the direct and indirect effects of BC. Emissions from these two sectors in China have near-zero net global forcings. Coal-fired power plants in both countries exert a negative forcing of about -30 mW m(-2) from production of sulfate. Aerosol forcings are largest locally, with direct forcings due to residential biofuel combustion of 580 mW m(-2) over India and 416 mW m(-2) over China, but they extend as far as North America, Europe, and the Arctic.
C1 [Streets, David G.; Lu, Zifeng] Argonne Natl Lab, Argonne, IL 60439 USA.
[Shindell, Drew T.; Faluvegi, Greg] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Shindell, Drew T.; Faluvegi, Greg] Columbia Univ, Columbia Earth Inst, New York, NY USA.
RP Streets, DG (reprint author), Argonne Natl Lab, Decis & Informat Sci Div, 9700 S Cass Ave, Argonne, IL 60439 USA.
EM dstreets@anl.gov
RI Lu, Zifeng/F-3266-2012; Shindell, Drew/D-4636-2012;
OI Streets, David/0000-0002-0223-1350
FU U.S. Department of Energy, Office of Fossil Energy; U.S. Department of
Energy [DE-AC02-06CH11357]; NASA Applied Sciences program
FX The work performed at the Argonne National Laboratory was funded by the
U.S. Department of Energy, Office of Fossil Energy. The authors
gratefully acknowledge the support of Thomas Grahame in that office.
Argonne National Laboratory is operated by UChicago Argonne, LLC, under
contract no. DE-AC02-06CH11357 with the U.S. Department of Energy. The
work performed at NASA/GISS was supported by the NASA Applied Sciences
program and used NASA Center for Climate Simulation resources at GSFC.
The authors thank George Milly for his assistance with the analysis of
model output.
NR 26
TC 7
Z9 7
U1 3
U2 34
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 AUG 28
PY 2013
VL 40
IS 16
BP 4409
EP 4414
DI 10.1002/grl.50805
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 219SI
UT WOS:000324529000052
ER
PT J
AU Suzuki, K
Golaz, JC
Stephens, GL
AF Suzuki, Kentaroh
Golaz, Jean-Christophe
Stephens, Graeme L.
TI Evaluating cloud tuning in a climate model with satellite observations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE aerosol indirect effect; cloud microphysics; model evaluation
ID PARAMETERIZATIONS; RADAR
AB This study examines the validity of a tunable cloud parameter, the threshold particle radius triggering the warm rain formation, in a climate model. Alternate values of the model's particular parameter within uncertainty have been shown to produce severely different historical temperature trends due to differing magnitude of aerosol indirect forcing. Three different threshold radii are evaluated against satellite observations in terms of the statistics depicting microphysical process signatures of the warm rain formation. The results show that the simulated temperature trend best matches to observed trend when the model adopts the threshold radius that worst reproduces satelliteobserved microphysical statistics and vice versa. This inconsistency between the bottomup processbased constraint and the topdown temperature trend constraint implies the presence of compensating errors in the model.
C1 [Suzuki, Kentaroh; Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Golaz, Jean-Christophe] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
RP Suzuki, K (reprint author), CALTECH, Jet Prop Lab, Mail Stop 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kentaro.suzuki@jpl.nasa.gov
RI Suzuki, Kentaroh/C-3624-2011; Golaz, Jean-Christophe/D-5007-2014
OI Golaz, Jean-Christophe/0000-0003-1616-5435
FU NASA [NNX07AR11G, NNX09AJ45G]
FX This study was carried out at Jet Propulsion Laboratory, California
Institute of Technology, under a contract with National Aeronautics and
Space Administration (NASA) and supported by NASA grants NNX07AR11G and
NNX09AJ45G. The CloudSat data products were provided by CloudSat Data
Processing Center at CIRA/Colorado State University.
NR 14
TC 12
Z9 12
U1 0
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 AUG 28
PY 2013
VL 40
IS 16
BP 4464
EP 4468
DI 10.1002/grl.50874
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 219SI
UT WOS:000324529000062
ER
PT J
AU Huang, XC
Fortenberry, RC
Lee, TJ
AF Huang, Xinchuan
Fortenberry, Ryan C.
Lee, Timothy J.
TI Protonated nitrous oxide, NNOH+: Fundamental vibrational frequencies and
spectroscopic constants from quartic force fields
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID MOLECULAR-STRUCTURE; ANALYTIC EVALUATION; ENERGY GRADIENTS;
WAVE-FUNCTIONS; BASIS-SETS; N2O; ISOTOPOLOGUES; MILLIMETER; SPECTRUM;
L-C3H+
AB The interstellar presence of protonated nitrous oxide has been suspected for some time. Using established high-accuracy quantum chemical techniques, spectroscopic constants and fundamental vibrational frequencies are provided for the lower energy O-protonated isomer of this cation and its deuterated isotopologue. The vibrationally-averaged B-0 and C-0 rotational constants are within 6 MHz of their experimental values and the D-J quartic distortion constants agree with experiment to within 3%. The known gas phase O-H stretch of NNOH+ is 3330.91 cm(-1), and the vibrational configuration interaction computed result is 3330.9 cm(-1). Other spectroscopic constants are also provided, as are the rest of the fundamental vibrational frequencies for NNOH+ and its deuterated isotopologue. This high-accuracy data should serve to better inform future observational or experimental studies of the rovibrational bands of protonated nitrous oxide in the interstellar medium and the laboratory. (C) 2013 AIP Publishing LLC.
C1 [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
[Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lee, TJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Xinchuan.Huang-1@nasa.gov; Timothy.J.Lee@nasa.gov
RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013
FU Oak Ridge Associated Universities through the NASA Postdoctoral Program;
NASA/SETI Institute [NNX12AG96A]; NASA [10-APRA10-0096]
FX X.H. and R.C.F. were supported by Oak Ridge Associated Universities
through the NASA Postdoctoral Program. The NASA/SETI Institute
Cooperative Agreement NNX12AG96A further funded the work undertaken by
X. H. T.J.L. and X. H. gratefully acknowledge funding from NASA Grant
No. 10-APRA10-0096. The CheMVP program, developed at the Center for
Computational Quantum Chemistry at the University of Georgia, was used
to create Fig. 1. Professor Wesley D. Allen is thanked for helpful
discussions regarding the use of the LINX/LINY coordinates for
quasilinear molecules and the use of INTDER program.
NR 46
TC 28
Z9 28
U1 1
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-9606
J9 J CHEM PHYS
JI J. Chem. Phys.
PD AUG 28
PY 2013
VL 139
IS 8
AR 084313
DI 10.1063/1.4819069
PG 7
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 211RO
UT WOS:000323928000039
PM 24007003
ER
PT J
AU Albayrak, A
Wei, J
Petrenko, M
Lynnes, C
Levy, RC
AF Albayrak, Arif
Wei, Jennifer
Petrenko, Maksym
Lynnes, Christopher
Levy, Robert C.
TI Global bias adjustment for MODIS aerosol optical thickness using neural
network
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE Aqua; Terra; MODIS; aerosol; bias adjustment; neural networks
ID ALGORITHMS; PRODUCTS; VALIDATION; AERONET; SYSTEM; LAND
AB Large uncertainties in calculating radiative forcings from aerosols due to their location, loading, and types pose a great challenge to global climate modeling. Trying to improve retrievals in a statistical manner normally requires detailed knowledge of uncertainty statistics and bias due to possible error sources such as different measurement viewing geometries, instrument calibration, and dynamically changing atmospheric and earth surface conditions. However, a priori estimates of these error sources are not, in general, available. The use of a neural network (NN) approach to compensate for biases and systematic errors of aerosol optical thickness (AOT) from the Moderate Resolution Imaging Spectrometer (MODIS) operational retrieval algorithm is explored. By utilizing the NN as an estimator, we can compensate against unknown sources of errors, nonlinearity in the data sets, and the presence of non-normal distributions. In this study, the highly accurate ground-based Aerosol Robotic Network (AERONET) measurements are used as the ground truth (GT). Our results show that the adjusted AOT with NN has decreased root mean square errors, improved correlations with GT data by 4% to 6%, and increased the number of NN-adjusted data falling within the published expected error envelope by similar to 10%. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.
C1 [Albayrak, Arif; Wei, Jennifer] ADNET Syst Inc, Rockville, MD 20852 USA.
[Albayrak, Arif; Wei, Jennifer; Petrenko, Maksym; Lynnes, Christopher; Levy, Robert C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Petrenko, Maksym] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Albayrak, A (reprint author), ADNET Syst Inc, Rockville, MD 20852 USA.
EM arif.albayrak@nasa.gov
RI Levy, Robert/M-7764-2013
OI Levy, Robert/0000-0002-8933-5303
NR 33
TC 4
Z9 4
U1 0
U2 11
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 1931-3195
J9 J APPL REMOTE SENS
JI J. Appl. Remote Sens.
PD AUG 28
PY 2013
VL 7
AR 073514
DI 10.1117/1.JRS.7.073514
PG 16
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 207KW
UT WOS:000323598600003
ER
PT J
AU Aartsen, MG
Abbasi, R
Abdou, Y
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Altmann, D
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Baum, V
Bay, R
Beatty, JJ
Bechet, S
Tjus, JB
Becker, KH
Benabderrahmane, ML
BenZvi, S
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Bertrand, D
Besson, DZ
Binder, G
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohaichuk, S
Bohm, C
Bose, D
Boser, S
Botner, O
Brayeur, L
Bretz, HP
Brown, AM
Bruijn, R
Brunner, J
Carson, M
Casey, J
Casier, M
Chirkin, D
Christov, A
Christy, B
Clark, K
Clevermann, F
Coenders, S
Cohen, S
Cowen, DF
Silva, AHC
Danninger, M
Daughhetee, J
Davis, JC
De Clercq, C
De Ridder, S
Desiati, P
de Vries, KD
de With, M
DeYoung, T
Diaz-Velez, JC
Dunkman, M
Eagan, R
Eberhardt, B
Eisch, J
Ellsworth, RW
Euler, S
Evenson, PA
Fadiran, O
Fazely, AR
Fedynitch, A
Feintzeig, J
Feusels, T
Filimonov, K
Finley, C
Fischer-Wasels, T
Flis, S
Franckowiak, A
Frantzen, K
Fuchs, T
Gaisser, TK
Gallagher, J
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Golup, G
Gonzalez, JG
Goodman, JA
Gora, D
Grandmont, DT
Grant, D
Gross, A
Ha, C
Ismail, AH
Hallen, P
Hallgren, A
Halzen, F
Hanson, K
Heereman, D
Heinen, D
Helbing, K
Hellauer, R
Hickford, S
Hill, GC
Hoffman, KD
Hoffmann, R
Homeier, A
Hoshina, K
Huelsnitz, W
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobi, E
Jacobsen, J
Jagielski, K
Japaridze, GS
Jero, K
Jlelati, O
Kaminsky, B
Kappes, A
Karg, T
Karle, A
Kelley, JL
Kiryluk, J
Klas, J
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krasberg, M
Krings, K
Kroll, G
Kunnen, J
Kurahashi, N
Kuwabara, T
Labare, M
Landsman, H
Larson, MJ
Lesiak-Bzdak, M
Leuermann, M
Leute, J
Lunemann, J
Maciias, O
Madsen, J
Maggi, G
Maruyama, R
Mase, K
Matis, HS
McNally, F
Meagher, K
Merck, M
Meures, T
Miarecki, S
Middell, E
Milke, N
Miller, J
Mohrmann, L
Montaruli, T
Morse, R
Nahnhauer, R
Naumann, U
Niederhausen, H
Nowicki, SC
Nygren, DR
Obertacke, A
Odrowski, S
Olivas, A
Omairat, A
O'Murchadha, A
Paul, L
Pepper, JA
de los Heros, CP
Pfendner, C
Pieloth, D
Pinat, E
Posselt, J
Price, PB
Przybylski, GT
Radel, L
Rameez, M
Rawlins, K
Redl, P
Reimann, R
Resconi, E
Rhode, W
Ribordy, M
Richman, M
Riedel, B
Rodrigues, JP
Rott, C
Ruhe, T
Ruzybayev, B
Ryckbosch, D
Saba, SM
Salameh, T
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Scheriau, F
Schmidt, T
Schmitz, M
Schoenen, S
Schoneberg, S
Schonwald, A
Schukraft, A
Schulte, L
Schulz, O
Seckel, D
Sestayo, Y
Seunarine, S
Shanidze, R
Sheremata, C
Smith, MWE
Soldin, D
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stasik, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strahler, EA
Strom, R
Sullivan, GW
Taavola, H
Taboada, I
Tamburro, A
Tepe, A
Ter-Antonyan, S
Tesic, G
Tilav, S
Toale, PA
Toscano, S
Unger, E
Usner, M
Vallecorsa, S
van Eijndhoven, N
van Overloop, A
van Santen, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Waldenmaier, T
Wallraff, M
Weaver, C
Wellons, M
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Williams, DR
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, C
Xu, DL
Xu, XW
Yanez, JP
Yodh, G
Yoshida, S
Zarzhitsky, P
Ziemann, J
Zierke, S
Zoll, M
AF Aartsen, M. G.
Abbasi, R.
Abdou, Y.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Altmann, D.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Baum, V.
Bay, R.
Beatty, J. J.
Bechet, S.
Tjus, J. Becker
Becker, K. -H.
Benabderrahmane, M. L.
BenZvi, S.
Berghaus, P.
Berley, D.
Bernardini, E.
Bernhard, A.
Bertrand, D.
Besson, D. Z.
Binder, G.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohaichuk, S.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Brayeur, L.
Bretz, H. -P.
Brown, A. M.
Bruijn, R.
Brunner, J.
Carson, M.
Casey, J.
Casier, M.
Chirkin, D.
Christov, A.
Christy, B.
Clark, K.
Clevermann, F.
Coenders, S.
Cohen, S.
Cowen, D. F.
Silva, A. H. Cruz
Danninger, M.
Daughhetee, J.
Davis, J. C.
De Clercq, C.
De Ridder, S.
Desiati, P.
de Vries, K. D.
de With, M.
DeYoung, T.
Diaz-Velez, J. C.
Dunkman, M.
Eagan, R.
Eberhardt, B.
Eisch, J.
Ellsworth, R. W.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Fedynitch, A.
Feintzeig, J.
Feusels, T.
Filimonov, K.
Finley, C.
Fischer-Wasels, T.
Flis, S.
Franckowiak, A.
Frantzen, K.
Fuchs, T.
Gaisser, T. K.
Gallagher, J.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Gonzalez, J. G.
Goodman, J. A.
Gora, D.
Grandmont, D. T.
Grant, D.
Gross, A.
Ha, C.
Ismail, A. Haj
Hallen, P.
Hallgren, A.
Halzen, F.
Hanson, K.
Heereman, D.
Heinen, D.
Helbing, K.
Hellauer, R.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Homeier, A.
Hoshina, K.
Huelsnitz, W.
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobi, E.
Jacobsen, J.
Jagielski, K.
Japaridze, G. S.
Jero, K.
Jlelati, O.
Kaminsky, B.
Kappes, A.
Karg, T.
Karle, A.
Kelley, J. L.
Kiryluk, J.
Klaes, J.
Klein, S. R.
Koehne, J. -H.
Kohnen, G.
Kolanoski, H.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Krasberg, M.
Krings, K.
Kroll, G.
Kunnen, J.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Landsman, H.
Larson, M. J.
Lesiak-Bzdak, M.
Leuermann, M.
Leute, J.
Luenemann, J.
Maciias, O.
Madsen, J.
Maggi, G.
Maruyama, R.
Mase, K.
Matis, H. S.
McNally, F.
Meagher, K.
Merck, M.
Meures, T.
Miarecki, S.
Middell, E.
Milke, N.
Miller, J.
Mohrmann, L.
Montaruli, T.
Morse, R.
Nahnhauer, R.
Naumann, U.
Niederhausen, H.
Nowicki, S. C.
Nygren, D. R.
Obertacke, A.
Odrowski, S.
Olivas, A.
Omairat, A.
O'Murchadha, A.
Paul, L.
Pepper, J. A.
de los Heros, C. Perez
Pfendner, C.
Pieloth, D.
Pinat, E.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Raedel, L.
Rameez, M.
Rawlins, K.
Redl, P.
Reimann, R.
Resconi, E.
Rhode, W.
Ribordy, M.
Richman, M.
Riedel, B.
Rodrigues, J. P.
Rott, C.
Ruhe, T.
Ruzybayev, B.
Ryckbosch, D.
Saba, S. M.
Salameh, T.
Sander, H. -G.
Santander, M.
Sarkar, S.
Schatto, K.
Scheriau, F.
Schmidt, T.
Schmitz, M.
Schoenen, S.
Schoeneberg, S.
Schoenwald, A.
Schukraft, A.
Schulte, L.
Schulz, O.
Seckel, D.
Sestayo, Y.
Seunarine, S.
Shanidze, R.
Sheremata, C.
Smith, M. W. E.
Soldin, D.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stasik, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strahler, E. A.
Strom, R.
Sullivan, G. W.
Taavola, H.
Taboada, I.
Tamburro, A.
Tepe, A.
Ter-Antonyan, S.
Tesic, G.
Tilav, S.
Toale, P. A.
Toscano, S.
Unger, E.
Usner, M.
Vallecorsa, S.
van Eijndhoven, N.
Van Overloop, A.
van Santen, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Weaver, Ch.
Wellons, M.
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, C.
Xu, D. L.
Xu, X. W.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
Ziemann, J.
Zierke, S.
Zoll, M.
CA IceCube Collaboration
TI Measurement of the cosmic ray energy spectrum with IceTop-73
SO PHYSICAL REVIEW D
LA English
DT Article
ID ICECUBE; ARRAY
AB We report on the measurement of the all-particle cosmic ray energy spectrum with the IceTop air shower array in the energy range from 1.58 PeV to 1.26 EeV. The IceTop air shower array is the surface component of the IceCube Neutrino Observatory at the geographical South Pole. The analysis was performed using only information from IceTop. The data used in this work were taken from June 1, 2010 to May 13, 2011. During that period the IceTop array consisted of 73 stations, compared to 81 in its final configuration. The measured spectrum exhibits a clear deviation from a single power law above the knee around 4 PeV and below 1 EeV. We observe spectral hardening around 18 PeV and steepening around 130 PeV.
C1 [Bissok, M.; Blumenthal, J.; Coenders, S.; Euler, S.; Hallen, P.; Heinen, D.; Jagielski, K.; Krings, K.; Leuermann, M.; Paul, L.; Raedel, L.; Reimann, R.; Schoenen, S.; Schukraft, A.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.; Zierke, S.] Rhein Westfal TH Aachen, Phys Inst 3, D-52056 Aachen, Germany.
[Aartsen, M. G.; Hill, G. C.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, 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.; 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.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Altmann, D.; de With, M.; Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Tjus, J. Becker; Fedynitch, A.; Saba, S. M.; Schoeneberg, S.; Unger, E.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Schulte, L.; Stasik, A.; Usner, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Bechet, S.; Bertrand, D.; Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Brussels, Fac Sci, B-1050 Brussels, Belgium.
[Bose, D.; Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; Golup, G.; Kunnen, J.; Maggi, G.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.; Brown, A. M.; Hickford, S.; Maciias, O.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Berley, D.; Blaufuss, E.; Christy, B.; Ellsworth, R. W.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Bohaichuk, S.; Grandmont, D. T.; Grant, D.; Nowicki, S. C.; Odrowski, S.; Sheremata, C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Aguilar, J. A.; Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[Abdou, Y.; Carson, M.; De Ridder, S.; Feusels, T.; Ismail, A. Haj; Jlelati, O.; Labare, M.; Ryckbosch, D.; Van Overloop, A.; 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.
[Bruijn, R.; Cohen, S.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Abbasi, R.; Ahlers, M.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kelley, J. L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Abbasi, R.; Ahlers, M.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kelley, J. L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Baum, V.; Eberhardt, B.; Koepke, L.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Bernhard, A.; Gross, A.; Leute, J.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany.
[Bai, X.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Bai, X.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Univ Stockholm, Dept Phys, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Univ Stockholm, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
[Larson, M. J.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Clark, K.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Eagan, R.; Koskinen, D. J.; Salameh, T.; Smith, M. W. E.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Boersma, D. J.; Botner, O.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Helbing, K.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Omairat, A.; Posselt, J.; Soldin, D.; Tepe, A.] Berg Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Ackermann, M.; Benabderrahmane, M. L.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Brunner, J.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Kaminsky, B.; Karg, T.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Spiering, C.; Stoessl, A.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Montaruli, T.] Sezione Ist Nazl Fis Nucl, Dipartimento Fis, I-70126 Bari, Italy.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ruzybayev, B (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
EM bahtiyar@udel.edu
RI Taavola, Henric/B-4497-2011; Wiebusch, Christopher/G-6490-2012;
Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Brunner,
Juergen/G-3540-2015; Aguilar Sanchez, Juan Antonio/H-4467-2015;
Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty,
James/D-9310-2011; Tjus, Julia/G-8145-2012
OI Taavola, Henric/0000-0002-2604-2810; Carson,
Michael/0000-0003-0400-7819; Perez de los Heros,
Carlos/0000-0002-2084-5866; Benabderrahmane, Mohamed
Lotfi/0000-0003-4410-5886; Wiebusch, Christopher/0000-0002-6418-3008;
Auffenberg, Jan/0000-0002-1185-9094; Koskinen,
David/0000-0002-0514-5917; Brunner, Juergen/0000-0002-5052-7236; Aguilar
Sanchez, Juan Antonio/0000-0003-2252-9514; Maruyama,
Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X; Beatty,
James/0000-0003-0481-4952; Rott, Carsten/0000-0002-6958-6033;
Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft,
Anne/0000-0002-9112-5479;
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; 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 program; 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)
FX We acknowledge 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, 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 program, 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).
NR 22
TC 44
Z9 44
U1 0
U2 17
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD AUG 28
PY 2013
VL 88
IS 4
AR 042004
DI 10.1103/PhysRevD.88.042004
PG 15
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 208WI
UT WOS:000323712300001
ER
PT J
AU Takahashi, H
Su, H
Jiang, JH
Luo, ZJ
Xie, SP
Hafner, J
AF Takahashi, Hanii
Su, Hui
Jiang, Jonathan H.
Luo, Zhengzhao Johnny
Xie, Shang-Ping
Hafner, Jan
TI Tropical water vapor variations during the 2006-2007 and 2009-2010 El
Ninos: Satellite observation and GFDL AM2.1 simulation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE tropical water vapor; El Nino; satellite observation; GCM simulation; CP
El Nino; interannual variability
ID SEA-SURFACE TEMPERATURES; DEEP CONVECTION; A-TRAIN; PACIFIC RIM; WARM
POOL; CLOUDS; MLS; HUMIDITY; MISSION; MODELS
AB Water vapor measurements from Aura Microwave Limb Sounder (MLS, above 300 hPa) and Aqua Atmospheric Infrared Sounder (AIRS, below 300 hPa) are analyzed to study the variations of moisture during the 2006-2007 and 2009-2010 El Ninos. The 2006-2007 El Nino is an East Pacific (EP) El Nino, while the 2009-2010 El Nino is a Central Pacific (CP) El Nino or El Nino Modoki. Results show that these two types of El Nino events produce different patterns of water vapor anomalies over the tropical ocean, approximately resembling the cloud anomalies shown in Su and Jiang (2013). Regression of water vapor anomalies onto the Nino-3.4 SST for the A-Train period shows a clear upper tropospheric amplification of the fractional water vapor change, i.e., the ratio of the change in specific humidity to the layer-averaged specific humidity. Furthermore, tropical water vapor anomalies in different circulation regimes are examined. It is shown that the variations of water vapor during the 2006-2007 El Nino are mainly controlled by the thermodynamic component, whereas both dynamic and thermodynamic components control the water vapor anomalies during the 2009-2010 El Nino. GFDL AM2.1 model simulations of water vapor and cloud anomalies for the two El Ninos are compared with the satellite observations. In general, the model approximately reproduces the water vapor anomalies on both zonal and meridional planes but it produces too strong a cloud response in the mid- and lower troposphere. The model fails to capture the dynamic component of water vapor anomalies, particularly over the Indian Ocean.
C1 [Takahashi, Hanii] CUNY, Grad Ctr, Program Earth & Environm Sci, New York, NY USA.
[Su, Hui; Jiang, Jonathan H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Luo, Zhengzhao Johnny] CUNY, Dept Earth & Atmospher Sci, New York, NY 10021 USA.
[Luo, Zhengzhao Johnny] CUNY, City Coll New York, CREST Inst, New York, NY 10021 USA.
[Xie, Shang-Ping] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Xie, Shang-Ping; Hafner, Jan] Univ Hawaii Manoa, Int Pacific Res Ctr, Honolulu, HI 96822 USA.
[Xie, Shang-Ping; Hafner, Jan] Univ Hawaii Manoa, Dept Meteorol, SOEST, Honolulu, HI 96822 USA.
RP Su, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Hui.Su@jpl.nasa.gov
RI Xie, Shang-Ping/C-1254-2009
OI Xie, Shang-Ping/0000-0002-3676-1325
FU NASA NEWS program; CloudSat-CALIPSO Science Team [NNX10AM31G]; SEAC4RS
Science Team [NNX12AC13G]; NSF; NOAA
FX HT acknowledges the JPL Graduate Fellowship program. The work was
conducted at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA. HS and JHJ thank the funding
support from NASA NEWS program. HT and ZJL are supported by
CloudSat-CALIPSO Science Team under grant NNX10AM31G and by SEAC4RS
Science Team under grant NNX12AC13G. SPX is supported by NSF and NOAA.
We greatly appreciate two reviewers' constructive comments that led to
the improvement of the manuscript.
NR 48
TC 7
Z9 7
U1 0
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2013
VL 118
IS 16
BP 8910
EP 8920
DI 10.1002/jgrd.50684
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 225AE
UT WOS:000324933900011
ER
PT J
AU Wen, GY
Marshak, A
Levy, RC
Remer, LA
Loeb, NG
Varnai, T
Cahalan, RF
AF Wen, Guoyong
Marshak, Alexander
Levy, Robert C.
Remer, Lorraine A.
Loeb, Norman G.
Varnai, Tamas
Cahalan, Robert F.
TI Improvement of MODIS aerosol retrievals near clouds
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE MODIS; aerosol; clouds; 3-D
ID ANGSTROM EXPONENT; WATER-VAPOR; DISTRIBUTIONS; SCATTERING; ALGORITHM;
ALBEDO
AB The retrieval of aerosol properties near clouds from reflected sunlight is challenging. Sunlight reflected from clouds can effectively enhance the reflectance in nearby clear regions. Ignoring cloud 3-D radiative effects can lead to large biases in aerosol retrievals, risking an incorrect interpretation of satellite observations on aerosol-cloud interaction. Earlier, we developed a simple model to compute the cloud-induced clear-sky radiance enhancement that is due to radiative interaction between boundary layer clouds and the molecular layer above. This paper focuses on the application and implementation of the correction algorithm. This is the first time that this method is being applied to a full Moderate Resolution Imaging Spectroradiometer (MODIS) granule. The process of the correction includes converting Clouds and the Earth's Radiant Energy System broadband flux to visible narrowband flux, computing the clear-sky radiance enhancement, and retrieving aerosol properties. We find that the correction leads to smaller values in aerosol optical depth (AOD), angstrom ngstrom exponent, and the small mode aerosol fraction of the total AOD. It also makes the average aerosol particle size larger near clouds than far away from clouds, which is more realistic than the opposite behavior observed in operational retrievals. We discuss issues in the current correction method as well as our plans to validate the algorithm.
C1 [Wen, Guoyong] Morgan State Univ, GESTAR, Baltimore, MD 21239 USA.
[Wen, Guoyong; Marshak, Alexander; Levy, Robert C.; Varnai, Tamas; Cahalan, Robert F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Remer, Lorraine A.; Varnai, Tamas] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Loeb, Norman G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Wen, GY (reprint author), NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA.
EM Guoyong.Wen-1@nasa.gov
RI Levy, Robert/M-7764-2013; Marshak, Alexander/D-5671-2012
OI Levy, Robert/0000-0002-8933-5303;
FU NASA Radiation Program; NASA CALIPSO project; NASA Terra/Aqua projects
FX We gratefully acknowledge support for this research by the NASA
Radiation Program managed by Hal Maring, the NASA CALIPSO project
supervised by David Considine, and the NASA Terra/Aqua projects managed
by Richard Eckman. We also thank Shana Mattoo for help with cloud mask
analysis, as well as Anthony Davis, Rob Wood, and Mark Vaughan for
insightful discussions and help.
NR 36
TC 6
Z9 8
U1 0
U2 17
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 AUG 27
PY 2013
VL 118
IS 16
BP 9168
EP 9181
DI 10.1002/jgrd.50617
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 225AE
UT WOS:000324933900029
ER
PT J
AU Cheng, AN
Xu, KM
AF Cheng, Anning
Xu, Kuan-Man
TI Diurnal variability of low clouds in the Southeast Pacific simulated by
a multiscale modeling framework model
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE diurnal variability; low clouds; multiscale modeling framework;
Southeast Pacific stratocumulus; third-order closure; diurnal cycle
mechanism
ID 3RD-ORDER TURBULENCE CLOSURES; BOUNDARY-LAYER STRUCTURE; CLIMATE SYSTEM
MODEL; LIQUID WATER PATH; VOCALS-REX; STRATOCUMULUS CLOUDS; SUBSEASONAL
VARIABILITY; RESOLVING MODEL; EASTERN PACIFIC; PART I
AB This study analyzes the diurnal variations of austral-spring stratocumulus clouds in the Southeast Pacific and their physical mechanisms from a global multiscale modeling framework (MMF) simulation. This MMF contains an advanced third-order turbulence closure in its cloud-resolving model component, helping it to realistically simulate boundary layer turbulence and low-level clouds. The main finding is that the MMF simulation can reproduce the spatial pattern of the diurnal variations of low clouds within the region, with the day-night cloud fraction (CF) differences ranging from 0.10 at 30 degrees off the shore to 0.40 near the shore. The diurnal phases and ranges of simulated liquid water path, CF, and surface cloud radiative effects agree well with available observations. The maximum CF occurs in the early morning and the minimum in the late afternoon over the open ocean. However, near the shore, the maximum/minimum CF anomalies are more variable. The spatial variability of the diurnal variations is attributed to the modulation of solar-forced variation by the orographically induced circulation. The solar radiation makes the lower cloud layer dissipated during the day, and clouds recover first there in the early evening, with the upper cloud layer changing relatively less in cloudiness. The southwestward propagating upsidence wave that is related to the orographical forcing modulates the CF anomalies near the shore. The orographically induced subsidence, however, extends too deeply into the boundary layer because of the model's unrealistically smooth topography, and it dissipates rather than enhances the stratocumulus near the shore between the late night and the following noon.
C1 [Cheng, Anning; Xu, Kuan-Man] NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Cheng, Anning] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Xu, KM (reprint author), NASA, Climate Sci Branch, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM Kuan-Man.Xu@nasa.gov
RI Xu, Kuan-Man/B-7557-2013
OI Xu, Kuan-Man/0000-0001-7851-2629
FU NASA Modeling, Analysis and Prediction program; DOE Atmospheric System
Research Program [DE-SC0005450]; NSF Science and Technology Center for
Multiscale Modeling of Atmospheric Processes (CMMAP) [ATM-0425247]
FX This work was supported by the NASA Modeling, Analysis and Prediction
program. This work was also partially supported by the DOE Atmospheric
System Research Program under interagency agreement DE-SC0005450 and the
NSF Science and Technology Center for Multiscale Modeling of Atmospheric
Processes (CMMAP), managed by Colorado State University, under
cooperative agreement ATM-0425247. The computation resources from the
NCAR BlueGene supercomputer were provided by the Teragrid organization.
Special thanks go to Marat Khairoutdinov of Stony Brook University for
providing SPCAM, and Zach Eitzen, Patrick Taylor, and David Painemal for
reading this manuscript.
NR 51
TC 7
Z9 7
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2013
VL 118
IS 16
BP 9191
EP 9208
DI 10.1002/jgrd.50683
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 225AE
UT WOS:000324933900031
ER
PT J
AU Thorsen, TJ
Fu, Q
Comstock, JM
Sivaraman, C
Vaughan, MA
Winker, DM
Turner, DD
AF Thorsen, Tyler J.
Fu, Qiang
Comstock, Jennifer M.
Sivaraman, Chitra
Vaughan, Mark A.
Winker, David M.
Turner, David D.
TI Macrophysical properties of tropical cirrus clouds from the CALIPSO
satellite and from ground-based micropulse and Raman lidars
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE CALIPSO; MPL; Raman; cirrus; tropics; diurnal
ID RADIATION MEASUREMENT PROGRAM; WATER-VAPOR; LOWER STRATOSPHERE; UPPER
TROPOSPHERE; MASS FLUXES; TROPOPAUSE; ALGORITHM; PROFILES; BALANCE;
PERFORMANCE
AB Lidar observations of cirrus cloud macrophysical properties over the U.S. Department of Energy Atmospheric Radiation Measurement (ARM) program Darwin, Australia, site are compared from the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) satellite, the ground-based ARM micropulse lidar (MPL), and the ARM Raman lidar (RL). Comparisons are made using the subset of profiles where the lidar beam is not fully attenuated. Daytime measurements using the RL are shown to be relatively unaffected by the solar background and are therefore suited for checking the validity of diurnal cycles. RL and CALIPSO cloud fraction profiles show good agreement while the MPL detects significantly less cirrus, particularly during the daytime. Both MPL and CALIPSO observations show that cirrus clouds occur less frequently during the day than at night at all altitudes. In contrast, the RL diurnal cycle is significantly different from zero only below about 11km; where it is of opposite sign (i.e., more clouds during the daytime). For cirrus geometrical thickness, the MPL and CALIPSO observations agree well and both data sets have significantly thinner clouds during the daytime than the RL. From the examination of hourly MPL and RL cirrus cloud thickness and through the application of daytime detection limits to all CALIPSO data, we find that the decreased MPL and CALIPSO cloud thickness during the daytime is very likely a result of increased daytime noise. This study highlights the significant improvement the RL provides (compared to the MPL) in the ARM program's ability to observe tropical cirrus clouds and will help improve our understanding of these clouds. The RL also provides a valuable ground-based lidar data set for the evaluation of CALIPSO observations.
C1 [Thorsen, Tyler J.; Fu, Qiang] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Comstock, Jennifer M.; Sivaraman, Chitra] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Vaughan, Mark A.; Winker, David M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Turner, David D.] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA.
RP Thorsen, TJ (reprint author), Univ Washington, Dept Atmospher Sci, ATG 408,Box 351640, Seattle, WA 98195 USA.
EM tylert@atmos.washington.edu
FU Office of Science (BER), U.S. Department of Energy [DE-FG02-09ER64769];
NASA [NNX13AN49G]; DOE ASR program; DOE ARM program
FX The micropulse and Raman lidar data sets were obtained from the ARM data
archive: www.archive.arm.gov. The CALIPSO data sets were obtained from
the NASA Langley Research Center Atmospheric Science Data Center. This
research was supported by the Office of Science (BER), U.S. Department
of Energy, grant DE-FG02-09ER64769 and by NASA grant NNX13AN49G. J.M.
Comstock was supported by both DOE ASR and ARM programs.
NR 49
TC 11
Z9 11
U1 0
U2 17
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 AUG 27
PY 2013
VL 118
IS 16
BP 9209
EP 9220
DI 10.1002/jgrd.50691
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 225AE
UT WOS:000324933900032
ER
PT J
AU Hsu, NC
Jeong, MJ
Bettenhausen, C
Sayer, AM
Hansell, R
Seftor, CS
Huang, J
Tsay, SC
AF Hsu, N. C.
Jeong, M. -J.
Bettenhausen, C.
Sayer, A. M.
Hansell, R.
Seftor, C. S.
Huang, J.
Tsay, S. -C.
TI Enhanced Deep Blue aerosol retrieval algorithm: The second generation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosol; satellite; retrieval
ID RESOLUTION IMAGING SPECTRORADIOMETER; LAND SURFACES; OPTICAL DEPTH;
MODIS; POLARIZATION; CAPABILITIES; REFLECTANCE; POLLUTION; CLOUDS; DUST
AB The aerosol products retrieved using the Moderate Resolution Imaging Spectroradiometer (MODIS) collection 5.1 Deep Blue algorithm have provided useful information about aerosol properties over bright-reflecting land surfaces, such as desert, semiarid, and urban regions. However, many components of the C5.1 retrieval algorithm needed to be improved; for example, the use of a static surface database to estimate surface reflectances. This is particularly important over regions of mixed vegetated and nonvegetated surfaces, which may undergo strong seasonal changes in land cover. In order to address this issue, we develop a hybrid approach, which takes advantage of the combination of precalculated surface reflectance database and normalized difference vegetation index in determining the surface reflectance for aerosol retrievals. As a result, the spatial coverage of aerosol data generated by the enhanced Deep Blue algorithm has been extended from the arid and semiarid regions to the entire land areas. In this paper, the changes made in the enhanced Deep Blue algorithm regarding the surface reflectance estimation, aerosol model selection, and cloud screening schemes for producing the MODIS collection 6 aerosol products are discussed. A similar approach has also been applied to the algorithm that generates the Sea-viewing Wide Field-of-view Sensor (SeaWiFS) Deep Blue products. Based upon our preliminary results of comparing the enhanced Deep Blue aerosol products with the Aerosol Robotic Network (AERONET) measurements, the expected error of the Deep Blue aerosol optical thickness (AOT) is estimated to be better than 0.05+20%. Using 10 AERONET sites with long-term time series, 79% of the best quality Deep Blue AOT values are found to fall within this expected error.
C1 [Hsu, N. C.; Bettenhausen, C.; Sayer, A. M.; Hansell, R.; Seftor, C. S.; Tsay, S. -C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jeong, M. -J.] Gangneung Wonju Natl Univ, Gangneung City, South Korea.
[Bettenhausen, C.; Seftor, C. S.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Sayer, A. M.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Greenbelt, MD USA.
[Hansell, R.; Huang, J.] UMD, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA.
[Huang, J.] NOAA, NESDIS, Ctr Satellite Applicat & Res, College Pk, MD USA.
RP Hsu, NC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Christina.Hsu@nasa.gov
RI Sayer, Andrew/H-2314-2012; Huang, Jingfeng/D-7336-2012; Tsay,
Si-Chee/J-1147-2014; Hansell, Richard/J-2065-2014
OI Sayer, Andrew/0000-0001-9149-1789; Huang, Jingfeng/0000-0002-8779-2922;
FU NASA EOS program
FX This work was supported by the NASA EOS program, managed by Hal Maring.
The authors gratefully acknowledge the MODIS Characterization Support
Team for their extensive efforts in maintaining the high radiometric
quality of MODIS level 1 data. Appreciations also extend to Jeremy
Warner and Rebecca Limbacher for their supports on the construction of
the Deep Blue surface database. We would also like to express our
gratitude to several AERONET PIs in establishing and maintaining the
long-term stations used in this investigation.
NR 37
TC 92
Z9 95
U1 7
U2 40
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 AUG 27
PY 2013
VL 118
IS 16
BP 9296
EP 9315
DI 10.1002/jgrd.50712
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 225AE
UT WOS:000324933900037
ER
PT J
AU Vergados, P
Mannucci, AJ
Su, H
AF Vergados, Panagiotis
Mannucci, Anthony J.
Su, Hui
TI A validation study for GPS radio occultation data with moist
thermodynamic structure of tropical cyclones
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE GPS; radio occultation; remote sensing; tropical cyclones; natural
hazards
ID GLOBAL POSITIONING SYSTEM; ASSIMILATION SYSTEM; WATER-VAPOR; RETRIEVAL;
AIRS
AB We exploit the cloud-penetrating capability and insensitivity to precipitation of the Global Positioning System radio occultation (GPSRO) technique to study the humidity environment of tropical cyclones (TCs). We focus in regions within and around the vicinity of TCs' eye, where infrared and microwave observations are difficult to acquire due to cloudiness and heavy precipitation. We use data from the National Hurricane Center TC Best Tracks to identify the location of North Atlantic TCs. The Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC) Data Analysis and Archive Center provides concurrent refractivity, temperature, and humidity measurements from the Challenging Minisatellite Payload and COSMIC missions and the European Centre for Medium-Range Weather Forecasts (ECMWF). The distribution of GPSRO-derived humidity profiles as functions of altitude and distance from the storms' center identifies a pronounced low-level inflow, characteristic of mature TCs, at distances between 50 and 90 km, which coincide with the area where the eyewall of TCs forms. We also capture wavelike structures resembling spiral rainbands beyond the eyewall. The distribution of water vapor as functions of altitude and TC intensity shows a decrease at all altitudes when a tropical system matures from a tropical depression to a Category 1 (Cat 1) hurricane. The water vapor gradually increases from Cat 2 to Cat 5 hurricanesa result that is also identified in ECMWF data sets and Atmospheric Infrared Sounder observations. We conclude that GPSRO data can contribute significantly to the understanding and modeling of the vertical structures of TCs.
C1 [Vergados, Panagiotis; Mannucci, Anthony J.; Su, Hui] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Vergados, P (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Panagiotis.Vergados@jpl.nasa.gov
FU National Aeronautics and Space Administration; NASA
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. P. Vergados acknowledges the NPP
program administered by the Oak Ridge Associated Universities (ORAU)
through a contract with NASA. We also thank the University Corporation
for Atmospheric Research (UCAR) for making the COSMIC and ECWMF data
sets publicly available. We also thank the three reviewers for providing
detailed and constructive comments, whose recommendations greatly
improved our manuscript.
NR 39
TC 5
Z9 5
U1 1
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2013
VL 118
IS 16
BP 9401
EP 9413
DI 10.1002/jgrd.50698
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 225AE
UT WOS:000324933900045
ER
PT J
AU Feng, WH
Marsh, DR
Chipperfield, MP
Janches, D
Hoffner, J
Yi, F
Plane, JMC
AF Feng, Wuhu
Marsh, Daniel R.
Chipperfield, Martyn P.
Janches, Diego
Hoeffner, Josef
Yi, Fan
Plane, John M. C.
TI A global atmospheric model of meteoric iron
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE mesosphere iron layer; WACCM; iron chemistry; transport; tides; gravity
wave
ID POLAR MESOSPHERIC CLOUDS; SPORADIC-E LAYERS; LIDAR OBSERVATIONS;
METALLIC-IONS; SODIUM LAYER; FE LAYERS; SEASONAL-VARIATIONS; NOCTILUCENT
CLOUDS; LOWER THERMOSPHERE; MIDDLE ATMOSPHERE
AB The first global model of meteoric iron in the atmosphere (WACCM-Fe) has been developed by combining three components: the Whole Atmosphere Community Climate Model (WACCM), a description of the neutral and ion-molecule chemistry of iron in the mesosphere and lower thermosphere (MLT), and a treatment of the injection of meteoric constituents into the atmosphere. The iron chemistry treats seven neutral and four ionized iron containing species with 30 neutral and ion-molecule reactions. The meteoric input function (MIF), which describes the injection of Fe as a function of height, latitude, and day, is precalculated from an astronomical model coupled to a chemical meteoric ablation model (CABMOD). This newly developed WACCM-Fe model has been evaluated against a number of available ground-based lidar observations and performs well in simulating the mesospheric atomic Fe layer. The model reproduces the strong positive correlation of temperature and Fe density around the Fe layer peak and the large anticorrelation around 100km. The diurnal tide has a significant effect in the middle of the layer, and the model also captures well the observed seasonal variations. However, the model overestimates the peak Fe(+)concentration compared with the limited rocket-borne mass spectrometer data available, although good agreement on the ion layer underside can be obtained by adjusting the rate coefficients for dissociative recombination of Fe-molecular ions with electrons. Sensitivity experiments with the same chemistry in a 1-D model are used to highlight significant remaining uncertainties in reaction rate coefficients, and to explore the dependence of the total Fe abundance on the MIF and rate of vertical transport.
C1 [Feng, Wuhu; Plane, John M. C.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England.
[Feng, Wuhu; Chipperfield, Martyn P.] Univ Leeds, Sch Earth & Environm, NCAS, Leeds LS2 9JT, W Yorkshire, England.
[Marsh, Daniel R.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Janches, Diego] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
[Hoeffner, Josef] Leibniz Inst Atmospher Phys, Kuhlungsborn, Germany.
[Yi, Fan] Wuhan Univ, Sch Elect Informat, Wuhan 430072, Peoples R China.
RP Plane, JMC (reprint author), Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England.
EM j.m.c.plane@leeds.ac.uk
RI Chipperfield, Martyn/H-6359-2013; Janches, Diego/D-4674-2012; Marsh,
Daniel/A-8406-2008; FENG, WUHU/B-8327-2008; Plane, John/C-7444-2015
OI Chipperfield, Martyn/0000-0002-6803-4149; Janches,
Diego/0000-0001-8615-5166; Marsh, Daniel/0000-0001-6699-494X; FENG,
WUHU/0000-0002-9907-9120; Plane, John/0000-0003-3648-6893
FU UK Natural Environment Research Council (NERC) [NE/G019487/1]; NSF
[ATM-05311464, ATM-0525655, ATM-0634650, AST-0908118]
FX This work was supported by the UK Natural Environment Research Council
(NERC grant NE/G019487/1). The MIF was developed under NSF grants
ATM-05311464, ATM-0525655, ATM-0634650, and AST-0908118 to NorthWest
Research Associates. The Fe lidar data for Urbana, Rothera, and South
Pole were provided by C. S. Gardner (University of Illinois at
Urbana-Champaign). We also thank R. J. Morris from Australian Antarctic
Division for supporting the lidar observations at Davis. CIRA data is
obtained via the British Atmospheric Data Centre. The authors also
acknowledge three anonymous reviewers for their useful comments.
NR 84
TC 38
Z9 38
U1 0
U2 20
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 AUG 27
PY 2013
VL 118
IS 16
BP 9456
EP 9474
DI 10.1002/jgrd.50708
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 225AE
UT WOS:000324933900049
ER
PT J
AU Auge, E
Sanchez, JE
Kiely, A
Blanes, I
Serra-Sagrista, J
AF Auge, Estanislau
Enrique Sanchez, Jose
Kiely, Aaron
Blanes, Ian
Serra-Sagrista, Joan
TI Performance impact of parameter tuning on the CCSDS-123 lossless multi-
and hyperspectral image compression standard
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE remote sensing; lossless image coding; predictive coding; multi- and
hyperspectral imagery; CCSDS 123.0-B-1; configuration parameters
AB Multi-spectral and hyperspectral image data payloads have large size and may be challenging to download from remote sensors. To alleviate this problem, such images can be effectively compressed using specially designed algorithms. The new CCSDS-123 standard has been developed to address onboard lossless coding of multi-spectral and hyperspectral images. The standard is based on the fast lossless algorithm, which is composed of a causal context-based prediction stage and an entropy-coding stage that utilizes Golomb power-of-two codes. Several parts of each of these two stages have adjustable parameters. CCSDS-123 provides satisfactory performance for a wide set of imagery acquired by various sensors; but end-users of a CCSDS-123 implementation may require assistance to select a suitable combination of parameters for a specific application scenario. To assist end-users, this paper investigates the performance of CCSDS-123 under different parameter combinations and addresses the selection of an adequate combination given a specific sensor. Experimental results suggest that prediction parameters have a greater impact on the compression performance than entropy-coding parameters. (C) 2013 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Auge, Estanislau; Enrique Sanchez, Jose; Blanes, Ian; Serra-Sagrista, Joan] Univ Autonoma Barcelona, Dept Informat & Commun Engn, UAB, E-08193 Barcelona, Spain.
[Kiely, Aaron] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
RP Auge, E (reprint author), Univ Autonoma Barcelona, Dept Informat & Commun Engn, UAB, Edifici Q, E-08193 Barcelona, Spain.
EM ian.blanes@uab.cat
RI Serra-Sagrista, Joan/B-2000-2009
OI Serra-Sagrista, Joan/0000-0003-4729-9292
FU Spanish Government; Fondo Europeo de Desarrollo Regional (FEDER);
Catalan Government [TIN2009-14426-C02-01, TIN2012-38102-C03-03,
2009-SGR-1224]
FX This work has been partially supported by the Spanish Government, by
Fondo Europeo de Desarrollo Regional (FEDER), and by the Catalan
Government, under grants TIN2009-14426-C02-01, TIN2012-38102-C03-03
(LIFE-VISION) and 2009-SGR-1224. The research conducted by A. Kiely was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. An earlier version of this work has been published in
the conference proceedings of the On-Board Payload Data Compression
Workshop 2012 by the European Space Agency and the Centre National
d'Etudes Spatiales.
NR 5
TC 3
Z9 3
U1 1
U2 14
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 1931-3195
J9 J APPL REMOTE SENS
JI J. Appl. Remote Sens.
PD AUG 26
PY 2013
VL 7
AR 074594
DI 10.1117/1JRS.7.074594
PG 16
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 206QQ
UT WOS:000323537600001
ER
PT J
AU Quattro, JM
Driggers, WB
Grady, JM
Ulrich, GF
Roberts, MA
AF Quattro, Joseph M.
Driggers, William B., III
Grady, James M.
Ulrich, Glenn F.
Roberts, Mark A.
TI Sphyrna gilberti sp nov., a new hammerhead shark (Carcharhiniformes,
Sphyrnidae) from the western Atlantic Ocean
SO ZOOTAXA
LA English
DT Article
DE Carolina hammerhead; cartilaginous fishes; Chondrichthyes; cryptic
species; Elasmobranchii
ID IDENTIFICATION; FISHES
AB Sphyrna gilberti sp. nov. is described based on 54 specimens collected in the coastal waters of South Carolina, U.S.A. Morphologically, S. gilberti sp. nov. is separable from S. lewini (Griffith & Smith 1834) only in the number of precaudal vertebrae. Due to rarity of specimens and the highly migratory behavior of most sphyrnids, the range of S. gilberti sp. nov. is unknown.
C1 [Quattro, Joseph M.; Roberts, Mark A.] Univ S Carolina, Dept Biol Sci, Marine Sci Program, Columbia, SC 29208 USA.
[Driggers, William B., III] Natl Marine Fisheries Serv, NOAA, Southeast Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA.
[Grady, James M.] Univ New Orleans, Dept Biol Sci, New Orleans, LA 70148 USA.
[Ulrich, Glenn F.] South Carolina Dept Nat Resources, Marine Resources Div, Charleston, SC 29412 USA.
RP Quattro, JM (reprint author), Univ S Carolina, Dept Biol Sci, Marine Sci Program, Columbia, SC 29208 USA.
EM JosephQ@mailbox.sc.edu
OI Roberts, Mark/0000-0002-0931-9363
NR 30
TC 6
Z9 7
U1 1
U2 25
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
J9 ZOOTAXA
JI Zootaxa
PD AUG 26
PY 2013
VL 3702
IS 2
BP 159
EP 178
PG 20
WC Zoology
SC Zoology
GA 205DU
UT WOS:000323422700005
PM 26146715
ER
PT J
AU Yamamoto, K
Matsuo, T
Shibai, H
Itoh, Y
Konishi, M
Sudo, J
Tanii, R
Fukagawa, M
Sumi, T
Kudo, T
Hashimoto, J
Kusakabe, N
Abe, L
Brandner, W
Brandt, TD
Carson, J
Currie, T
Egner, SE
Feldt, M
Goto, M
Grady, C
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, K
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, GR
Kuzuhara, M
Kwon, J
McElwain, M
Miyama, S
Morino, JI
Moro-Martin, A
Nishikawa, J
Nishimura, T
Pyo, TS
Serabyn, E
Suto, H
Suzuki, R
Takami, M
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Wisniewski, J
Watanabe, M
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Yamamoto, Kodai
Matsuo, Taro
Shibai, Hiroshi
Itoh, Yoichi
Konishi, Mihoko
Sudo, Jun
Tanii, Ryoko
Fukagawa, Misato
Sumi, Takahiro
Kudo, Tomoyuki
Hashimoto, Jun
Kusakabe, Nobuhiko
Abe, Lyu
Brandner, Wolfgang
Brandt, Timothy D.
Carson, Joseph
Currie, Thayne
Egner, Sebastian E.
Feldt, Markus
Goto, Miwa
Grady, Carol
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko
Henning, Thomas
Hodapp, Klaus
Ishii, Miki
Iye, Masanori
Janson, Markus
Kandori, Ryo
Knapp, Gillian R.
Kuzuhara, Masayuki
Kwon, Jungmi
McElwain, Mike
Miyama, Shoken
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishikawa, June
Nishimura, Tetsuo
Pyo, Tae-Soo
Serabyn, Eugene
Suto, Hiroshi
Suzuki, Ryuji
Takami, Michihiro
Takato, Naruhisa
Terada, Hiroshi
Thalmann, Christian
Tomono, Daigo
Turner, Edwin L.
Wisniewski, John
Watanabe, Makoto
Yamada, Toru
Takami, Hideki
Usuda, Tomonori
Tamura, Motohide
TI Direct Imaging Search for Extrasolar Planets in the Pleiades
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE infrared: stars; methods: statistical; stars: low-mass, brown dwarfs;
stars: planetary systems; techniques: high angular resolution
ID LOW-MASS STARS; ORBITING HR 8799; GIANT PLANETS; OPEN CLUSTERS; BROWN
DWARFS; GRAVITATIONAL-INSTABILITY; PROTOPLANETARY DISKS; EVOLUTIONARY
MODELS; CIRCUMSTELLAR DISK; YOUNG JUPITERS
AB We carried out an imaging survey for extrasolar planets around stars in the Pleiades (125 Myr, 135 pc) in the H and K-S bands using HiCIAO combined with adaptive optics, AO188, on the Subaru telescope. We found 13 companion candidates fainter than 14.5 mag in the H band around 9 stars. Five of these 13 were confirmed to be background stars by measurement of their proper motion. One was not found in the second epoch observation, and thus was not a background or companion object. One had multi-epoch images, but the precision of its proper motion was not sufficient to conclude whether it was a background object. Four other candidates are waiting for second-epoch observations to determine their proper motion. Finally, the remaining two were confirmed to be 60 M-J brown dwarf companions orbiting around HD 23514 (G0) and HII 1348 (K5), respectively, as had been reported in previous studies. In our observations, the average detection limit for a point source was 20.3 mag in the H band beyond 1.'' 5 from the central star. On the basis of this detection limit, we calculated the detection efficiency to be 90% for a planet with 6 to 12 Jovian masses and a semi-major axis of 50-1000 AU. For this reason we extrapolated the distribution of the planet mass and the semi-major axis derived from radial velocity observations, and adopted the planet evolution model Baraffe et al. (2003, A&A, 402, 701). Since there was no detection of a planet, we estimated the frequency of such planets to be less than 17.9% (2 sigma) around one star of the Pleiades cluster.
C1 [Yamamoto, Kodai; Shibai, Hiroshi; Konishi, Mihoko; Sudo, Jun; Fukagawa, Misato; Sumi, Takahiro] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Matsuo, Taro] Kyoto Univ, Fac Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Itoh, Yoichi] Nishi Harima Astron Observ, Sayo, Hyogo 6795313, Japan.
[Tanii, Ryoko] Kobe Univ, Grad Sch Sci, Nada Ku, Kobe, Hyogo 6578501, Japan.
[Kudo, Tomoyuki; Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko; Ishii, Miki; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo; Usuda, Tomonori] Subaru Telescope, Hilo, HI 96720 USA.
[Hashimoto, Jun; Kusakabe, Nobuhiko; Hayashi, Masahiko; Iye, Masanori; Kandori, Ryo; Kuzuhara, Masayuki; Kwon, Jungmi; Morino, Jun-Ichi; Nishikawa, June; Suto, Hiroshi; Takami, Hideki] Natl Astron Observ, Mitaka, Tokyo 1818588, Japan.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06300 Nice, France.
[Brandner, Wolfgang; Feldt, Markus; Goto, Miwa; Henning, Thomas; Thalmann, Christian] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Brandt, Timothy D.; Janson, Markus; Knapp, Gillian R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Carson, Joseph; Turner, Edwin L.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Currie, Thayne] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 1A1, Canada.
[Grady, Carol] Eureka Sci, Oakland, CA 96002 USA.
[Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Hodapp, Klaus] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Kwon, Jungmi] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
[McElwain, Mike] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Miyama, Shoken] Hiroshima Univ, Off President, Hiroshima 7398511, Japan.
[Moro-Martin, Amaya] CSIC, INTA, CAB, Dept Astrofis, Madrid 28850, Spain.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Suzuki, Ryuji] TMT Observ Corp, Pasadena, CA 91105 USA.
[Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Wisniewski, John] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[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 Yamamoto, K (reprint author), Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan.
EM yamamoto@iral.ess.sci.osaka-u.ac.jp; matsuo@kusastro.kyoto-u.ac.jp;
shibai@iral.ess.sci.osaka-u.ac.jp; yitoh@nhao.jp;
konishi@iral.ess.sci.osaka-u.ac.jp; sudo@iral.ess.sci.osaka-u.ac.jp;
misato@iral.ess.sci.osaka-u.ac.jp; sumi@iral.ess.sciosaka-u.ac.jp
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
NR 68
TC 18
Z9 18
U1 0
U2 1
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 AUG 25
PY 2013
VL 65
IS 4
AR 90
DI 10.1093/pasj/65.4.90
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 298MP
UT WOS:000330328300021
ER
PT J
AU Minazzoli, O
Hees, A
AF Minazzoli, Olivier
Hees, Aurelien
TI Intrinsic Solar System decoupling of a scalar-tensor theory with a
universal coupling between the scalar field and the matter Lagrangian
SO PHYSICAL REVIEW D
LA English
DT Article
ID EQUIVALENCE PRINCIPLE; GENERAL-RELATIVITY; INFLATIONARY UNIVERSE;
COSMOLOGICAL PROBLEMS; MASSIVE BODIES; STRING THEORY; DARK ENERGY;
GRAVITY; PULSAR; SPACE
AB In this Communication, we present a class of Brans-Dicke-like theories with a universal coupling between the scalar field and the matter Lagrangian. We show this class of theories naturally exhibits a decoupling mechanism between the scalar field and matter. As a consequence, this coupling leads to almost the same phenomenology as general relativity in the Solar System: the trajectories of massive bodies and the light propagation differ from general relativity only at the second post-Newtonian order. Deviations from general relativity are beyond present detection capabilities. However, this class of theories predicts a deviation of the gravitational redshift at a level detectable by the future ACES and STE/QUEST missions.
C1 [Minazzoli, Olivier] Univ Nice Sophia Antipolis, CNRS, UMR ARTEMIS, Observ Cote Azur, F-06304 Nice 4, France.
[Hees, Aurelien] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Minazzoli, O (reprint author), Univ Nice Sophia Antipolis, CNRS, UMR ARTEMIS, Observ Cote Azur, BP4229, F-06304 Nice 4, France.
OI Minazzoli, Olivier/0000-0002-3151-7593
FU Belgian American Educational Foundation (BAEF); Gustave-Boel-Sofina
"Plateforme pour l'Education et le Talent"
FX The authors want to thank Tiberiu Harko, Viktor Toth and John Moffat for
their useful comments and the anonymous referees for their valuable
suggestions and comments. The research described in this paper was
partially carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. A. H. acknowledges support from the Belgian
American Educational Foundation (BAEF) and from the Gustave-Boel-Sofina
"Plateforme pour l'Education et le Talent."
NR 90
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U2 2
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 AUG 23
PY 2013
VL 88
IS 4
AR 041504
DI 10.1103/PhysRevD.88.041504
PG 5
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 207CA
UT WOS:000323573200002
ER
PT J
AU Smith, SJ
Adams, JS
Bailey, CN
Bandler, SR
Busch, SE
Chervenak, JA
Eckart, ME
Finkbeiner, FM
Kilbourne, CA
Kelley, RL
Lee, SJ
Porst, JP
Porter, FS
Sadleir, JE
AF Smith, Stephen J.
Adams, Joseph S.
Bailey, Catherine N.
Bandler, Simon R.
Busch, Sarah E.
Chervenak, James A.
Eckart, Megan E.
Finkbeiner, Fred M.
Kilbourne, Caroline A.
Kelley, Richard L.
Lee, Sang-Jun
Porst, Jan-Patrick
Porter, Frederick S.
Sadleir, John E.
TI Implications of weak-link behavior on the performance of Mo/Au bilayer
transition-edge sensors
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID LOW-TEMPERATURE DETECTORS; X-RAY MICROCALORIMETERS; CRYOGENIC DETECTORS;
NOISE; SPECTROMETER; CALORIMETER; RESOLUTION; REDUCTION; PHYSICS
AB Understanding the physical properties of the superconducting-to-normal transition is fundamental for optimizing the design and performance of transition-edge sensors (TESs). Recent critical current I-C measurements of square Mo/Au bilayer structures show that they act as weak superconducting links, exhibiting oscillatory, Fraunhofer-like behavior with applied magnetic field. In this paper, we investigate the implications of this behavior for TES x-ray detectors operated in the resistive transition. These devices include normal metal features used for absorber attachment and suppression of detector noise. We present extensive measurements of I-C as a function of temperature T and field B, which show a complex temperature and current evolution when compared with the behavior expected from a simple geometry. We introduce a resistively shunted junction model for describing the TES resistive transition as a function of current I, temperature T, and magnetic field B. From this model, we calculate the R(T, I, B) transition and the logarithmic resistance sensitivity with respect to T and I (alpha and beta, respectively), as a function of applied magnetic field and operating point within the resistive transition. Different examples are presented to illustrate the role of critical current on the transition parameters, and results are qualitatively compared with measurements. Results show that the important device parameters alpha and beta exhibit oscillatory behavior with applied magnetic field due to the modulation of the critical current. This in turn affects the signal responsivity and noise, and the predicted energy resolution. These results show the significance of the critical current in determining the performance of TESs and how externally applied and self-induced magnetic fields can affect the transition and, thus, hold promise for future optimization. (C) 2013 AIP Publishing LLC.
C1 [Smith, Stephen J.; Adams, Joseph S.; Bandler, Simon R.; Chervenak, James A.; Eckart, Megan E.; Finkbeiner, Fred M.; Kilbourne, Caroline A.; Kelley, Richard L.; Porst, Jan-Patrick; Porter, Frederick S.; Sadleir, John E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Smith, Stephen J.; Adams, Joseph S.; Eckart, Megan E.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Bailey, Catherine N.; Busch, Sarah E.; Lee, Sang-Jun] NASA, Goddard Space Flight Ctr, NASA Postdoctoral Program, Greenbelt, MD 20771 USA.
[Bandler, Simon R.] CRESST, College Pk, MD 20742 USA.
[Bandler, Simon R.] Univ Maryland, College Pk, MD 20742 USA.
[Finkbeiner, Fred M.] Wyle Informat Syst, Mclean, VA 22102 USA.
[Porst, Jan-Patrick] CRESST, Columbia, MD 21044 USA.
[Porst, Jan-Patrick] USRA, Columbia, MD 21044 USA.
RP Smith, SJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Smith, Stephen/B-1256-2008; Bandler, Simon/A-6258-2010; Lee, Sang
Jun/A-3892-2015; Porter, Frederick/D-3501-2012
OI Smith, Stephen/0000-0003-4096-4675; Bandler, Simon/0000-0002-5112-8106;
Lee, Sang Jun/0000-0002-8199-3993; Porter, Frederick/0000-0002-6374-1119
FU Goddard Space Flight Center; NASA; National Aeronautics and Space
Administration through its Astrophysics Research and Analysis Program
FX This research was in part supported by appointment (C. N. Bailey, S. E.
Busch, S. J. Lee) to the NASA Postdoctoral Program at Goddard Space
Flight Center, administered by Oak Ridge Associated Universities through
a contract with NASA. We thank Jorn Beyer (PTB-Berlin) for providing the
SQUIDs used in this work. This material is based upon work supported by
the National Aeronautics and Space Administration under an award issued
through its Astrophysics Research and Analysis Program.
NR 42
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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 AUG 21
PY 2013
VL 114
IS 7
AR 074513
DI 10.1063/1.4818917
PG 24
WC Physics, Applied
SC Physics
GA 206HV
UT WOS:000323510900083
ER
PT J
AU Alexander, DM
Stern, D
Del Moro, A
Lansbury, GB
Assef, RJ
Aird, J
Ajello, M
Ballantyne, DR
Bauer, FE
Boggs, SE
Brandt, WN
Christensen, FE
Civano, F
Comastri, A
Craig, WW
Elvis, M
Grefenstette, BW
Hailey, CJ
Harrison, FA
Hickox, RC
Luo, B
Madsen, KK
Mullaney, JR
Perri, M
Puccetti, S
Saez, C
Treister, E
Urry, CM
Zhang, WW
Bridge, CR
Eisenhardt, PRM
Gonzalez, AH
Miller, SH
Tsai, CW
AF Alexander, D. M.
Stern, D.
Del Moro, A.
Lansbury, G. B.
Assef, R. J.
Aird, J.
Ajello, M.
Ballantyne, D. R.
Bauer, F. E.
Boggs, S. E.
Brandt, W. N.
Christensen, F. E.
Civano, F.
Comastri, A.
Craig, W. W.
Elvis, M.
Grefenstette, B. W.
Hailey, C. J.
Harrison, F. A.
Hickox, R. C.
Luo, B.
Madsen, K. K.
Mullaney, J. R.
Perri, M.
Puccetti, S.
Saez, C.
Treister, E.
Urry, C. M.
Zhang, W. W.
Bridge, C. R.
Eisenhardt, P. R. M.
Gonzalez, A. H.
Miller, S. H.
Tsai, C. W.
TI THE NuSTAR EXTRAGALACTIC SURVEY: A FIRST SENSITIVE LOOK AT THE
HIGH-ENERGY COSMIC X-RAY BACKGROUND POPULATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: high-redshift; infrared: galaxies; X-rays:
diffuse background; X-rays: general
ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; BL-LACERTAE OBJECTS; MS SOURCE
CATALOGS; ALL-SKY SURVEY; RESOLUTION SPECTRAL TEMPLATES; HOST-GALAXY
PROPERTIES; STAR-FORMING GALAXIES; POINT-SOURCE CATALOGS; HEAVILY
OBSCURED AGN
AB We report on the first 10 identifications of sources serendipitously detected by the Nuclear Spectroscopic Telescope Array (NuSTAR) to provide the first sensitive census of the cosmic X-ray background source population at greater than or similar to 10 keV. We find that these NuSTAR-detected sources are approximate to 100 times fainter than those previously detected at greater than or similar to 10 keV and have a broad range in redshift and luminosity (z = 0.020-2.923 and L10-40 keV approximate to 4 x 10(41)-5 x 10(45) erg s(-1)); the median redshift and luminosity are z approximate to 0.7 and L10-40 keV approximate to 3 x 10(44) erg s(-1), respectively. We characterize these sources on the basis of broad-band approximate to 0.5-32 keV spectroscopy, optical spectroscopy, and broad-band ultraviolet-to-mid-infrared spectral energy distribution analyses. We find that the dominant source population is quasars with L10-40 keV > 10(44) erg s(-1), of which approximate to 50% are obscured with N-H greater than or similar to 10(22) cm(-2). However, none of the 10 NuSTAR sources are Compton thick (N-H greater than or similar to 10(24) cm(-2)) and we place a 90% confidence upper limit on the fraction of Compton-thick quasars (L10-40 keV > 10(44) erg s(-1)) selected at greater than or similar to 10 keV of less than or similar to 33% over the redshift range z = 0.5-1.1. We jointly fitted the rest-frame approximate to 10-40 keV data for all of the non-beamed sources with L10-40 keV > 10(43) erg s(-1) to constrain the average strength of reflection; we find R < 1.4 for Gamma = 1.8, broadly consistent with that found for local active galactic nuclei (AGNs) observed at greater than or similar to 10 keV. We also constrain the host-galaxy masses and find a median stellar mass of approximate to 10(11) M-circle dot, a factor approximate to 5 times higher than the median stellar mass of nearby high-energy selected AGNs, which may be at least partially driven by the order of magnitude higher X-ray luminosities of the NuSTAR sources. Within the low source-statistic limitations of our study, our results suggest that the overall properties of the NuSTAR sources are broadly similar to those of nearby high-energy selected AGNs but scaled up in luminosity and mass.
C1 [Alexander, D. M.; Del Moro, A.; Lansbury, G. B.; Aird, J.; Mullaney, J. R.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Stern, D.; Assef, R. J.; Eisenhardt, P. R. M.; Tsai, C. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ajello, M.; Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Bauer, F. E.; Saez, C.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Civano, F.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA.
[Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Grefenstette, B. W.; Harrison, F. A.; Madsen, K. K.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Hailey, C. J.] Columbia Astrophys Lab, Columbia, NY 10027 USA.
[Perri, M.; Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Perri, M.; Puccetti, S.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Urry, C. M.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bridge, C. R.; Miller, S. H.] CALTECH, Pasadena, CA 91125 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
RP Alexander, DM (reprint author), Univ Durham, Dept Phys, Durham DH1 3LE, England.
RI Urry, Claudia/G-7381-2011; Boggs, Steven/E-4170-2015; Brandt,
William/N-2844-2015; Comastri, Andrea/O-9543-2015;
OI Alexander, David/0000-0002-5896-6313; Puccetti,
Simonetta/0000-0002-2734-7835; Urry, Claudia/0000-0002-0745-9792; Boggs,
Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453;
Comastri, Andrea/0000-0003-3451-9970; Perri, Matteo/0000-0003-3613-4409
FU Leverhulme Trust; Science and Technology Facilities Council (STFC); SAO
grant [GO2-13164X]; NASA Postdoctoral Program at the Jet Propulsion
Laboratory; NSF award [AST 1008067]; Center of Excellence in
Astrophysics and Associated Technologies [PFB 06/2007]; Anillo project
[ACT1101]; FONDECYT [1101024, 1120061]; Caltech NuSTAR [44A-1092750];
NASA ADP grant [NNX10AC99G]; ASI/INAF grant [I/037/12/0]; CONICYT-Chile
under grant FONDECYT [3120198]; NASA [NNG08FD60C]; National Aeronautics
and Space Administration
FX We acknowledge financial support from the Leverhulme Trust (D.M.A. and
J.R.M.), the Science and Technology Facilities Council (STFC; D.M.A.,
A.D.M., and G.B.L.), the SAO grant GO2-13164X (M.A.), NASA Postdoctoral
Program at the Jet Propulsion Laboratory (R.J.A.), NSF award AST 1008067
(D.R.B.), Center of Excellence in Astrophysics and Associated
Technologies (PFB 06/2007; F.E.B. and E.T.), the Anillo project ACT1101
(F.E.B. and E.T.), FONDECYT Regular 1101024 (F.E.B.), Caltech NuSTAR
subcontract 44A-1092750 (W.N.B. and B.L.), NASA ADP grant NNX10AC99G
(W.N.B. and B.L.), ASI/INAF grant I/037/12/0 (A.C. and S.P.),
CONICYT-Chile under grant FONDECYT 3120198 (C.S.), and FONDECYT regular
grant 1120061 (E.T.). We thank the referee for a constructive and
positive report. We also thank Michael Koss for the discussion of
Swift-BAT results, and Mark Brodwin, Daniel Gettings, John Gizis,
Richard Walters, Jingwen Wu, and Dominika Wylezalek for supporting the
ground-based follow-up observations. 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 (NuSTAR-DAS) jointly developed by the ASI Science Data Center
(ASDC, Italy) and the California Institute of Technology (USA).
NR 136
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U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2013
VL 773
IS 2
AR 125
DI 10.1088/0004-637X/773/2/125
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205EU
UT WOS:000323426100044
ER
PT J
AU Anfinogentov, S
Nakariakov, VM
Mathioudakis, M
Van Doorsselaere, T
Kowalski, AF
AF Anfinogentov, S.
Nakariakov, V. M.
Mathioudakis, M.
Van Doorsselaere, T.
Kowalski, A. F.
TI THE DECAYING LONG-PERIOD OSCILLATION OF A STELLAR MEGAFLARE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: flare; stars: low-mass; stars: oscillations; Sun: oscillations
ID DOPPLER-SHIFT OSCILLATIONS; BRAGG CRYSTAL SPECTROMETER; WHITE-LIGHT
FLARE; X-RAY; CORONAL LOOPS; MICROWAVE EMISSION; SOLAR-FLARES; YZ-CMI;
AD LEO; WAVES
AB We analyze and interpret the oscillatory signal in the decay phase of the U-band light curve of a stellar megaflare observed on 2009 January 16 on the dM4.5e star YZ CMi. The oscillation is well approximated by an exponentially decaying harmonic function. The period of the oscillation is found to be 32 minutes, the decay time about 46 minutes, and the relative amplitude 15%. As this observational signature is typical of the longitudinal oscillations observed in solar flares at extreme ultraviolet and radio wavelengths, associated with standing slow magnetoacoustic waves, we suggest that this megaflare may be of a similar nature. In this scenario, macroscopic variations of the plasma parameters in the oscillations modulate the ejection of non-thermal electrons. The phase speed of the longitudinal (slow magnetoacoustic) waves in the flaring loop or arcade, the tube speed, of about 230 km s(-1) would require a loop length of about 200 Mm. Other mechanisms, such as standing kink oscillations, are also considered.
C1 [Anfinogentov, S.] Inst Solar Terr Phys, Irkutsk, Russia.
[Nakariakov, V. M.] Univ Warwick, Ctr Fus Space & Astrophys, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Nakariakov, V. M.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi, South Korea.
[Nakariakov, V. M.] Russian Acad Sci, Cent Astron Observ Pulkovo, St Petersburg 196140, Russia.
[Mathioudakis, M.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Van Doorsselaere, T.] Katholieke Univ Leuven, Dept Math, Ctr Math Plasma Astrophys, B-3001 Louvain, Belgium.
[Kowalski, A. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Anfinogentov, S (reprint author), Inst Solar Terr Phys, Irkutsk, Russia.
EM anfinogentov@iszf.irk.ru
RI Lee, SungHwan/O-2563-2013; Van Doorsselaere, Tom/B-4967-2008;
Nakariakov, Valery/E-2375-2013; Anfinogentov, Sergey/A-6836-2014
OI Van Doorsselaere, Tom/0000-0001-9628-4113; Nakariakov,
Valery/0000-0001-6423-8286; Anfinogentov, Sergey/0000-0002-1107-7420
FU FP7 Marie Curie RadioSun project [PIRSES-GA-2011-295272]; European
Research Council [321141]; Russian Ministry of Education and Science
[8524, 16.518.11.7065, 02.740.11.0576]; Russian Foundation of Basic
Research [12-02-33110-mol-a-ved, 12-02-31746-mol-a, 13-02-00044-a,
13-02-90472-ukr-f-a]; Kyung Hee University; FWO-Vlaanderen; Framework
Programme 7 [276808]; Leverhulme Trust [F/00203/X]
FX The work is supported by the FP7 Marie Curie PIRSES-GA-2011-295272
RadioSun project, the European Research Council under the SeismoSun
Research Project No. 321141 (VMN), the Russian Ministry of Education and
Science project No. 8524, State Contracts 16.518.11.7065 and
02.740.11.0576, the Russian Foundation of Basic Research under grants
12-02-33110-mol-a-ved, 12-02-31746-mol-a, 13-02-00044-a and
13-02-90472-ukr-f-a, and the Kyung Hee University International
Scholarship (V.M.N.). T.V.D. has received funding from an Odysseus grant
of the FWO-Vlaanderen and from the Framework Programme 7 under grant
agreement 276808. M.M. is grateful to the Leverhulme Trust for grant
F/00203/X.
NR 59
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2013
VL 773
IS 2
AR 156
DI 10.1088/0004-637X/773/2/156
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205EU
UT WOS:000323426100075
ER
PT J
AU Ballard, S
Charbonneau, D
Fressin, F
Torres, G
Irwin, J
Desert, JM
Newton, E
Mann, AW
Ciardi, DR
Crepp, JR
Henze, CE
Bryson, ST
Howell, SB
Horch, EP
Everett, ME
Shporer, A
AF Ballard, Sarah
Charbonneau, David
Fressin, Francois
Torres, Guillermo
Irwin, Jonathan
Desert, Jean-Michel
Newton, Elisabeth
Mann, Andrew W.
Ciardi, David R.
Crepp, Justin R.
Henze, Christopher E.
Bryson, Stephen T.
Howell, Steven B.
Horch, Elliott P.
Everett, Mark E.
Shporer, Avi
TI EXOPLANET CHARACTERIZATION BY PROXY: A TRANSITING 2.15 R-circle plus
PLANET NEAR THE HABITABLE ZONE OF THE LATE K DWARF KEPLER-61
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; planetary systems; stars: individual (Kepler-61, KOI 1361, KIC
6960913)
ID LOW-MASS STARS; INFRARED TELESCOPE FACILITY; EFFECTIVE TEMPERATURE
SCALE; FULLY CONVECTIVE STARS; HUBBLE-SPACE-TELESCOPE; MAIN-SEQUENCE
STARS; SUN-LIKE STAR; TIMING VARIATIONS; LIGHT-CURVE; EXTRASOLAR PLANET
AB We present the validation and characterization of Kepler-61b: a 2.15 R-circle plus planet orbiting near the inner edge of the habitable zone of a low-mass star. Our characterization of the host star Kepler-61 is based upon a comparison with a set of spectroscopically similar stars with directly measured radii and temperatures. We apply a stellar prior drawn from the weighted mean of these properties, in tandem with the Kepler photometry, to infer a planetary radius for Kepler-61b of 2.15 +/- 0.13 R-circle plus and an equilibrium temperature of 273 +/- 13 K (given its period of 59.87756 +/- 0.00020 days and assuming a planetary albedo of 0.3). The technique of leveraging the physical properties of nearby "proxy" stars allows for an independent check on stellar characterization via the traditional measurements with stellar spectra and evolutionary models. In this case, such a check had implications for the putative habitability of Kepler-61b: the planet is 10% warmer and larger than inferred from K-band spectral characterization. From the Kepler photometry, we estimate a stellar rotation period of 36 days, which implies a stellar age of >1 Gyr. We summarize the evidence for the planetary nature of the Kepler-61 transit signal, which we conclude is 30,000 times more likely to be due to a planet than a blend scenario. Finally, we discuss possible compositions for Kepler-61b with a comparison to theoretical models as well as to known exoplanets with similar radii and dynamically measured masses.
C1 [Ballard, Sarah; Charbonneau, David; Fressin, Francois; Torres, Guillermo; Irwin, Jonathan; Newton, Elisabeth] Univ Washington, Seattle, WA 98195 USA.
[Desert, Jean-Michel; Crepp, Justin R.; Shporer, Avi] CALTECH, Pasadena, CA 91125 USA.
[Mann, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Henze, Christopher E.; Bryson, Stephen T.; Howell, Steven B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Horch, Elliott P.] So Connecticut State Univ, New Haven, CT 06515 USA.
[Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
RP Ballard, S (reprint author), Univ Washington, Seattle, WA 98195 USA.
EM sarahba@uw.edu
FU NASA; NASA's Science Mission Directorate; National Aeronautics and Space
Administration under the Exoplanet Exploration Program
FX We thank Perry Berlind and Mike Calkins at the Fred Lawrence Whipple
Observatory for gathering the FAST spectra of Kepler-61 and GJ 380. We
thank Courtney Dressing for applying the methodology of Dressing &
Charbonneau (2013) to deduce the physical properties of Kepler-61 and
sharing these values with us. We thank Philip Muirhead, Katherine
Hamren, Everett Schlawin, Barbara Rojas-Ayala, Kevin Covey, and James
Lloyd for gathering, reducing, and sharing the TripleSpec K-band
spectrum of Kepler-61. We thank the Spitzer team at the Infrared
Processing and Analysis Center in Pasadena, California, and in
particular Nancy Silbermann for scheduling the Spitzer observations of
this program. This work was performed in part under contract with the
California Institute of Technology (Caltech) funded by NASA through the
Sagan Fellowship Program. It was conducted with 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. This work is also based on observations made with
Kepler, which was competitively selected as the tenth Discovery mission.
Funding for this mission is provided by NASA's Science Mission
Directorate. The authors would like to thank the many people who
generously gave so much their time to make this Mission a success. 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.
NR 103
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U2 39
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2013
VL 773
IS 2
AR 98
DI 10.1088/0004-637X/773/2/98
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205EU
UT WOS:000323426100017
ER
PT J
AU Hudson, RL
Loeffler, MJ
AF Hudson, Reggie L.
Loeffler, Mark J.
TI KETENE FORMATION IN INTERSTELLAR ICES: A LABORATORY STUDY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; astrochemistry; ISM: molecules; molecular data; molecular
processes
ID ABSOLUTE INFRARED INTENSITIES; RARE-GAS MATRICES; VINYL ALCOHOL;
WATER-ICE; RADIATION-CHEMISTRY; UV PHOTOCHEMISTRY; ORGANIC-MOLECULES;
CARBON SUBOXIDE; OXYGEN-ATOMS; SOLID ARGON
AB The formation of ketene (H2CCO, ethenone) in polar and apolar ices was studied with in situ 0.8 MeV proton irradiation, far-UV photolysis, and infrared spectroscopic analyses at 10-20 K. Using isotopically enriched reagents, unequivocal evidence was obtained for ketene synthesis in H2O-rich and CO2-rich ices, and several reaction products were identified. Results from scavenging experiments suggested that ketene was formed by free-radical pathways, as opposed to acid-base processes or redox reactions. Finally, we use our results to draw conclusions about the formation and stability of ketene in the interstellar medium.
C1 [Hudson, Reggie L.; Loeffler, Mark J.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hudson, RL (reprint author), NASA, Astrochem Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Reggie.Hudson@NASA.gov
RI Loeffler, Mark/C-9477-2012
NR 72
TC 2
Z9 2
U1 1
U2 23
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2013
VL 773
IS 2
AR 109
DI 10.1088/0004-637X/773/2/109
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205EU
UT WOS:000323426100028
ER
PT J
AU Lionello, R
Winebarger, AR
Mok, Y
Linker, JA
Mikic, Z
AF Lionello, Roberto
Winebarger, Amy R.
Mok, Yung
Linker, Jon A.
Mikic, Zoran
TI THERMAL NON-EQUILIBRIUM REVISITED: A HEATING MODEL FOR CORONAL LOOPS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: UV radiation
ID ACTIVE-REGION LOOPS; EMISSION-MEASURE PROFILES; ATOMIC DATABASE; 3
DIMENSIONS; PROMINENCES; DYNAMICS; EXPLORER; TRACE; TEMPERATURE; CHIANTI
AB The location and frequency of events that heat the million-degree corona are still a matter of debate. One potential heating scenario is that the energy release is effectively steady and highly localized at the footpoints of coronal structures. Such an energy deposition drives thermal non-equilibrium solutions in the hydrodynamic equations in longer loops. This heating scenario was considered and discarded by Klimchuk et al. on the basis of their one-dimensional simulations as incapable of reproducing observational characteristics of loops. In this paper, we use three-dimensional simulations to generate synthetic emission images, from which we select and analyze six loops. The main differences between our model and that of Klimchuk et al. concern (1) dimensionality, (2) resolution, (3) geometrical properties of the loops, (4) heating function, and (5) radiative function. We find evidence, in this small set of simulated loops, that the evolution of the light curves, the variation of temperature along the loops, the density profile, and the absence of small-scale structures are compatible with the characteristics of observed loops. We conclude that quasi-steady footpoint heating that drives thermal non-equilibrium solutions cannot yet be ruled out as a viable heating scenario for EUV loops.
C1 [Lionello, Roberto; Linker, Jon A.; Mikic, Zoran] Predict Sci Inc, San Diego, CA 92121 USA.
[Winebarger, Amy R.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Mok, Yung] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
RP Lionello, R (reprint author), Predict Sci Inc, 9990 Mesa Rim Rd,Ste 170, San Diego, CA 92121 USA.
EM lionel@predsci.com; amy.r.winebarger@nasa.gov; ymok@uci.edu;
linkerj@predsci.com; mikicz@predsci.com
FU NASA's LWS Program; NASA's Heliophysics Theory Program; NSF's Strategic
Capabilities Program; NSF's Center for Integrated Space Weather
Modeling; AFOSR
FX We are grateful to Dr. James A. Klimchuk for many helpful discussions.
This work was supported by NASA's LWS and Heliophysics Theory Programs,
NSF's Strategic Capabilities Program and the Center for Integrated Space
Weather Modeling, and AFOSR. Computational support provided by NASA's
NAS division at Ames, and by NSF at the TACC.
NR 44
TC 16
Z9 16
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 AUG 20
PY 2013
VL 773
IS 2
AR 134
DI 10.1088/0004-637X/773/2/134
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205EU
UT WOS:000323426100053
ER
PT J
AU Mahmoodifar, S
Strohmayer, T
AF Mahmoodifar, Simin
Strohmayer, Tod
TI UPPER BOUNDS ON r-MODE AMPLITUDES FROM OBSERVATIONS OF LOW-MASS X-RAY
BINARY NEUTRON STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dense matter; gravitational waves; stars: neutron; stars: oscillations;
stars: rotation; X-rays: binaries
ID GRAVITATIONAL-WAVE EMISSION; ROTATING RELATIVISTIC STARS; MAXIMUM SPIN
FREQUENCY; SAX J1808.4-3658; MILLISECOND PULSAR; INSTABILITY; CRUSTS;
CONSTRAINTS; STATE; OSCILLATIONS
AB We present upper limits on the amplitude of r-mode oscillations and gravitational-radiation-induced spin-down rates in low-mass X-ray binary neutron stars, under the assumption that the quiescent neutron star luminosity is powered by dissipation from a steady-state r-mode. For masses <2M(circle dot) we find dimensionless r-mode amplitudes in the range from about 1 x 10(-8) to 1.5 x 10(-6). For the accreting millisecond X-ray pulsar sources with known quiescent spin-down rates, these limits suggest that less than or similar to 1% of the observed rate can be due to an unstable r-mode. Interestingly, the source with the highest amplitude limit, NGC 6440, could have an r-mode spin-down rate comparable to the observed, quiescent rate for SAX J1808-3658. Thus, quiescent spin-down measurements for this source would be particularly interesting. For all sources considered here, our amplitude limits suggest that gravitational wave signals are likely too weak for detection with Advanced LIGO. Our highest mass model (2.21 M-circle dot) can support enhanced, direct Urca neutrino emission in the core and thus can have higher r-mode amplitudes. Indeed, the inferred r-mode spin-down rates at these higher amplitudes are inconsistent with the observed spin-down rates for some of the sources, such as IGR J00291+5934 and XTE J1751-305. In the absence of other significant sources of internal heat, these results could be used to place an upper limit on the masses of these sources if they were made of hadronic matter, or alternatively it could be used to probe the existence of exotic matter in them if their masses were known.
C1 [Mahmoodifar, Simin] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Strohmayer, Tod] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Mahmoodifar, S (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
FU U.S. Department of Energy [DEFG02- 93ER-40762]
FX S.M. thanks Mark Alford, Andrew Cumming, Cole Miller, and Kai Schwenzer
for helpful discussions. T.S. acknowledges NASA's support for
high-energy astrophysics. S.M. acknowledges the support of the U.S.
Department of Energy through grant No. DEFG02- 93ER-40762.
NR 59
TC 22
Z9 22
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2013
VL 773
IS 2
AR 140
DI 10.1088/0004-637X/773/2/140
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205EU
UT WOS:000323426100059
ER
PT J
AU Mikic, Z
Lionello, R
Mok, Y
Linker, JA
Winebarger, AR
AF Mikic, Zoran
Lionello, Roberto
Mok, Yung
Linker, Jon A.
Winebarger, Amy R.
TI THE IMPORTANCE OF GEOMETRIC EFFECTS IN CORONAL LOOP MODELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE hydrodynamics; Sun: atmosphere; Sun: corona; Sun: transition region;
Sun: UV radiation
ID SOFT-X-RAY; SOLAR ACTIVE REGIONS; AB-INITIO APPROACH; TRANSITION-REGION;
ATOMIC DATABASE; THERMAL NONEQUILIBRIUM; EMISSION-LINES; HEATING
PROBLEM; 3 DIMENSIONS; CHIANTI
AB We systematically investigate the effects of geometrical assumptions in one-dimensional (1D) models of coronal loops. Many investigations of coronal loops have been based on restrictive assumptions, including symmetry in the loop shape and heating profile, and a uniform cross-sectional area. Starting with a solution for a symmetric uniform-area loop with uniform heating, we gradually relax these restrictive assumptions to consider the effects of nonuniform area, nonuniform heating, a nonsymmetric loop shape, and nonsymmetric heating, to show that the character of the solutions can change in important ways. We find that loops with nonuniform cross-sectional area are more likely to experience thermal nonequilibrium, and that they produce significantly enhanced coronal emission, compared with their uniform-area counterparts. We identify a process of incomplete condensation in loops experiencing thermal nonequilibrium during which the coronal parts of loops never fully cool to chromospheric temperatures. These solutions are characterized by persistent siphon flows. Their properties agree with observations (Lionello et al.) and may not suffer from the drawbacks that led Klimchuk et al. to conclude that thermal nonequilibrium is not consistent with observations. We show that our 1D results are qualitatively similar to those seen in a three-dimensional model of an active region. Our results suggest that thermal nonequilibrium may play an important role in the behavior of coronal loops, and that its dismissal by Klimchuk et al., whose model suffered from some of the restrictive assumptions we described, may have been premature.
C1 [Mikic, Zoran; Lionello, Roberto; Linker, Jon A.] Predict Sci Inc, San Diego, CA 92121 USA.
[Mok, Yung] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Winebarger, Amy R.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Mikic, Z (reprint author), Predict Sci Inc, San Diego, CA 92121 USA.
FU NASA's LWS Program; NASA's Heliophysics Theory Program; NSF's Strategic
Capabilities Program; Center for Integrated Space Weather Modeling;
AFOSR
FX We are grateful to Drs. Jim Klimchuk and Judy Karpen for many helpful
discussions. This work was supported by NASA's LWS and Heliophysics
Theory Programs, NSF's Strategic Capabilities Program and the Center for
Integrated Space Weather Modeling, and AFOSR. This paper is an outgrowth
of the participation of Z.M. and R.L. in the 2011 "Loops Workshop."
NR 58
TC 24
Z9 24
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 AUG 20
PY 2013
VL 773
IS 2
AR 94
DI 10.1088/0004-637X/773/2/94
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205EU
UT WOS:000323426100013
ER
PT J
AU Scowcroft, V
Freedman, WL
Madore, BF
Monson, AJ
Persson, SE
Seibert, M
Rigby, JR
Melbourne, J
AF Scowcroft, Victoria
Freedman, Wendy L.
Madore, Barry F.
Monson, Andrew J.
Persson, S. E.
Seibert, Mark
Rigby, Jane R.
Melbourne, Jason
TI THE CARNEGIE HUBBLE PROGRAM: THE INFRARED LEAVITT LAW IN IC 1613
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: distances and redshifts; galaxies: individual (IC 1613);
infrared: galaxies; infrared: stars; stars: variables: Cepheids
ID PERIOD-LUMINOSITY RELATION; CEPHEID DISTANCE SCALE;
LARGE-MAGELLANIC-CLOUD; RED GIANT BRANCH; SPACE-TELESCOPE;
VARIABLE-STARS; CCD PHOTOMETRY; MU-M; METALLICITY; GALAXIES
AB We have observed the dwarf galaxy IC 1613, at multiple epochs in the mid-infrared using Spitzer and contemporaneously in the near-infrared using the new FourStar near-infrared camera on Magellan. We have constructed Cepheid period-luminosity relations in the J, H, K-s, [3.6] and [4.5] bands and have used the run of their apparent distance moduli as a function of wavelength to derive the line-of-sight reddening and distance to IC 1613. Using a nine-band fit, we find E(B - V) = 0.05 +/- 0.01 mag and an extinction-corrected distance modulus of mu(0) = 24.29 +/- 0.03(statistical) +/- 0.03(systematic) mag. By comparing our multi-band and [3.6] distance moduli to results from the tip of the red giant branch and red clump distance indicators, we find that metallicity has no measurable effect on Cepheid distances at 3.6 mu m in the metallicity range -1.0 <= [Fe/H] <= 0.2, hence derivations of the Hubble constant at this wavelength require no correction for metallicity.
C1 [Scowcroft, Victoria; Freedman, Wendy L.; Madore, Barry F.; Monson, Andrew J.; Persson, S. E.; Seibert, Mark] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Rigby, Jane R.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Melbourne, Jason] CALTECH, Caltech Opt Observ, Div Phys Math & Astron, Pasadena, CA 91125 USA.
RP Scowcroft, V (reprint author), Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA.
EM vs@obs.carnegiescience.edu; wendy@obs.carnegiescience.edu;
barry@obs.carnegiescience.edu; amonson@obs.carnegiescience.edu;
persson@obs.carnegiescience.edu; mseibert@obs.carnegiescience.edu;
jane.r.rigby@nasa.gov; jmel@caltech.edu
RI Rigby, Jane/D-4588-2012
OI Rigby, Jane/0000-0002-7627-6551
FU National Aeronautics and Space Administration
FX 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.
NR 44
TC 8
Z9 8
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2013
VL 773
IS 2
AR 106
DI 10.1088/0004-637X/773/2/106
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205EU
UT WOS:000323426100025
ER
PT J
AU Strohmayer, TE
Kallman, TR
AF Strohmayer, T. E.
Kallman, T. R.
TI ON THE STATISTICAL ANALYSIS OF X-RAY POLARIZATION MEASUREMENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; methods: statistical; polarization; X-rays:
general
ID CRAB-NEBULA; SENSITIVITY; POLARIMETRY; ASTRONOMY; PULSAR; NOISE
AB In many polarimetry applications, including observations in the X-ray band, the measurement of a polarization signal can be reduced to the detection and quantification of a deviation from uniformity of a distribution of measured angles of the form A + B cos(2)(phi - phi(0)) (0 < phi < pi). We explore the statistics of such polarization measurements using Monte Carlo simulations and chi(2) fitting methods. We compare our results to those derived using the traditional probability density used to characterize polarization measurements and quantify how they deviate as the intrinsic modulation amplitude grows. We derive relations for the number of counts required to reach a given detection level (parameterized by beta the "number of sigma's" of the measurement) appropriate for measuring the modulation amplitude a by itself (single interesting parameter case) or jointly with the position angle phi (two interesting parameters case). We show that for the former case, when the intrinsic amplitude is equal to the well-known minimum detectable polarization, (MDP) it is, on average, detected at the 3 sigma level. For the latter case, when one requires a joint measurement at the same confidence level, then more counts are needed than what was required to achieve the MDP level. This additional factor is amplitude-dependent, but is approximate to 2.2 for intrinsic amplitudes less than about 20%. It decreases slowly with amplitude and is approximate to 1.8 when the amplitude is 50%. We find that the position angle uncertainty at 1 sigma confidence is well described by the relation sigma(phi) = 28.degrees 5/beta.
C1 [Strohmayer, T. E.; Kallman, T. R.] NASA, Xray Astrophys Lab, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Strohmayer, TE (reprint author), NASA, Xray Astrophys Lab, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 21
TC 12
Z9 12
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2013
VL 773
IS 2
AR 103
DI 10.1088/0004-637X/773/2/103
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205EU
UT WOS:000323426100022
ER
PT J
AU Wahhaj, Z
Liu, MC
Nielsen, EL
Biller, BA
Hayward, TL
Close, LM
Males, JR
Skemer, A
Ftaclas, C
Chun, M
Thatte, N
Tecza, M
Shkolnik, EL
Kuchner, M
Reid, IN
Dal Pino, EMD
Alencar, SHP
Gregorio-Hetem, J
Boss, A
Lin, DNC
Toomey, DW
AF Wahhaj, Zahed
Liu, Michael C.
Nielsen, Eric L.
Biller, Beth A.
Hayward, Thomas L.
Close, Laird M.
Males, Jared R.
Skemer, Andrew
Ftaclas, Christ
Chun, Mark
Thatte, Niranjan
Tecza, Matthias
Shkolnik, Evgenya L.
Kuchner, Marc
Reid, I. Neill
de Gouveia Dal Pino, Elisabete M.
Alencar, Silvia H. P.
Gregorio-Hetem, Jane
Boss, Alan
Lin, Douglas N. C.
Toomey, Douglas W.
TI THE GEMINI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF GIANT PLANETS
AROUND DEBRIS DISK STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; circumstellar matter; infrared: planetary systems;
instrumentation: adaptive optics; methods: statistical; planetary
systems
ID SUN-LIKE STARS; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; BETA-PICTORIS;
NEARBY STARS; HR 8799; EXTRASOLAR PLANETS; MASSIVE PLANETS;
SPACE-TELESCOPE; SOUTHERN STARS
AB We have completed a high-contrast direct imaging survey for giant planets around 57 debris disk stars as part of the Gemini NICI Planet-Finding Campaign. We achieved median H-band contrasts of 12.4 mag at 0.'' 5 and 14.1 mag at 1 '' separation. Follow-up observations of the 66 candidates with projected separation <500 AU show that all of them are background objects. To establish statistical constraints on the underlying giant planet population based on our imaging data, we have developed a new Bayesian formalism that incorporates (1) non-detections, (2) single-epoch candidates, (3) astrometric and (4) photometric information, and (5) the possibility of multiple planets per star to constrain the planet population. Our formalism allows us to include in our analysis the previously known beta Pictoris and the HR 8799 planets. Our results show at 95% confidence that <13% of debris disk stars have a >= 5 M-Jup planet beyond 80 AU, and <21% of debris disk stars have a >= 3 M-Jup planet outside of 40 AU, based on hot-start evolutionary models. We model the population of directly imaged planets as d(2)N/dMda proportional to m(alpha)a(beta), where m is planet mass and a is orbital semi-major axis (with a maximum value of a(max)). We find that beta < -0.8 and/or alpha > 1.7. Likewise, we find that beta < -0.8 and/or a(max) < 200 AU. For the case where the planet frequency rises sharply with mass (alpha > 1.7), this occurs because all the planets detected to date have masses above 5 M-Jup, but planets of lower mass could easily have been detected by our search. If we ignore the beta Pic and HR 8799 planets (should they belong to a rare and distinct group), we find that <20% of debris disk stars have a >= 3 M-Jup planet beyond 10 AU, and beta < -0.8 and/or alpha < -1.5. Likewise, beta < -0.8 and/or a(max) < 125 AU. Our Bayesian constraints are not strong enough to reveal any dependence of the planet frequency on stellar host mass. Studies of transition disks have suggested that about 20% of stars are undergoing planet formation; our non-detections at large separations show that planets with orbital separation >40 AU and planet masses >3 M-Jup do not carve the central holes in these disks.
C1 [Wahhaj, Zahed] European So Observ, Santiago, Chile.
[Liu, Michael C.; Nielsen, Eric L.; Ftaclas, Christ; Chun, Mark] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Biller, Beth A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Hayward, Thomas L.] AURA, Southern Operat Ctr, Gemini Observ, La Serena, Chile.
[Close, Laird M.; Males, Jared R.; Skemer, Andrew] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Thatte, Niranjan; Tecza, Matthias] Univ Oxford, Dept Astron, Oxford OX1 3RH, England.
[Shkolnik, Evgenya L.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Kuchner, Marc] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Reid, I. Neill] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[de Gouveia Dal Pino, Elisabete M.; Gregorio-Hetem, Jane] Univ Sao Paulo, IAG, Dept Astron, BR-05508900 Sao Paulo, Brazil.
[Alencar, Silvia H. P.] Univ Fed Minas Gerais, ICEx, Dept Fis, BR-30270901 Belo Horizonte, MG, Brazil.
[Boss, Alan] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Lin, Douglas N. C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Toomey, Douglas W.] Mauna Kea Infrared LLC, Hilo, HI 96720 USA.
RP Wahhaj, Z (reprint author), European So Observ, Alonso de Cordova 3107,Casilla 19001, Santiago, Chile.
RI Gregorio-Hetem, Jane/A-5924-2013; Alencar, Silvia/C-2803-2013; de
Gouveia Dal Pino, Elisabete/H-9560-2013;
OI de Gouveia Dal Pino, Elisabete/0000-0001-8058-4752; Biller,
Beth/0000-0003-4614-7035; Skemer, Andrew/0000-0001-6098-3924; Nielsen,
Eric/0000-0001-6975-9056
FU NSF [AST-0713881, AST-0709484]
FX This work was supported in part by NSF grants AST-0713881 and
AST-0709484. The Gemini Observatory 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 Science and Technology
Facilities Council (United Kingdom), the National Research Council
(Canada), CONICYT (Chile), the Australian Research Council (Australia),
CNPq (Brazil), and CONICET (Argentina). Our research has employed the
2MASS data products, NASA's Astrophysical Data System, and the SIMBAD
database operated at CDS, Strasbourg, France. We thank Ruobing Dong and
Lucas Cieza for discussions on the importance of transition disks to
planet formation.
NR 86
TC 46
Z9 46
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2013
VL 773
IS 2
AR 179
DI 10.1088/0004-637X/773/2/179
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205EU
UT WOS:000323426100098
ER
PT J
AU Wehrle, AE
Wiita, PJ
Unwin, SC
Di Lorenzo, P
Revalski, M
Silano, D
Sprague, D
AF Wehrle, Ann E.
Wiita, Paul J.
Unwin, Stephen C.
Di Lorenzo, Paolo
Revalski, Mitchell
Silano, Daniel
Sprague, Dan
TI KEPLER PHOTOMETRY OF FOUR RADIO-LOUD ACTIVE GALACTIC NUCLEI IN 2010-2012
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; galaxies: active;
galaxies: Seyfert; quasars: general
ID ACCRETION DISK MODELS; FAST TEV VARIABILITY; DIGITAL SKY SURVEY; RAY
LIGHT CURVES; OPTICAL VARIABILITY; PERIODIC OSCILLATIONS; QUASAR
VARIABILITY; QUIET QUASARS; S5 0716+714; BLAZARS
AB We have used Kepler photometry to characterize variability in four radio-loud active galactic nuclei (AGN; three quasars and one object tentatively identified as a Seyfert 1.5 galaxy) on timescales from minutes to months, comparable to the light crossing time of the accretion disk around the central supermassive black hole or the base of the relativistic jet. Kepler's almost continuous observations provide much better temporal coverage than is possible from ground-based observations. We report the first such data analyzed for quasars. We have constructed power spectral densities using eight Kepler quarters of long-cadence (30-minute) data for three AGN, six quarters for one AGN and two quarters of short-cadence (1-minute) data for all four AGN. On timescales longer than about 0.2-0.6 days, we find red noise with mean power-law slopes ranging from -1.8 to -1.2, consistent with the variability originating in turbulence either behind a shock or within an accretion disk. Each AGN has a range of red noise slopes which vary slightly by month and quarter of observation. No quasi-periodic oscillations of astrophysical origin were detected. We detected flares of several days long when brightness increased by 3%-7% in two objects. No flares on timescales of minutes to hours were detected. Our observations imply that the duty cycle for enhanced activity in these radio-loud AGN is small. These well-sampled AGN light curves provide an impetus to develop more detailed models of turbulence in jets and instabilities in accretion disks.
C1 [Wehrle, Ann E.] Space Sci Inst, Boulder, CO 80301 USA.
[Wiita, Paul J.; Di Lorenzo, Paolo; Revalski, Mitchell; Silano, Daniel; Sprague, Dan] Coll New Jersey, Dept Phys, Ewing, NJ 08628 USA.
[Unwin, Stephen C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wehrle, AE (reprint author), Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
EM awehrle@spacescience.org
OI Wiita, Paul/0000-0002-1029-3746
FU NASA Kepler Guest Observer Program [NNX11B90G, NNX12AC83G]; Mentored
Undergraduate Summer Experience program; National Aeronautics and Space
Administration; NASA [NAS5-26555]; NASA Office of Space Science
[NNX09AF08G]
FX We thank Martin Still and Tom Barclay (Kepler Science Center, NASA Ames
Research Center), Jeff Kolodziejczak (Kepler Mission, Marshall Space
Flight Center), Rick Edelson (University of Maryland Baltimore County),
Mike Carini (Western Kentucky University), Paul Smith (Steward
Observatory), Rob Olling (UMBC), and Dave Monet (USNO) for helpful
discussions. We acknowledge support from the NASA Kepler Guest Observer
Program through grants to A. E. Wehrle (NNX11B90G and NNX12AC83G). The
TCNJ group acknowledges additional support from the Mentored
Undergraduate Summer Experience program. This work made use of PyKe, a
software package for the reduction and analysis of Kepler data. This
open source software project is developed and distributed by the NASA
Kepler Guest Observer Office. 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. 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.
NR 67
TC 12
Z9 12
U1 0
U2 7
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 AUG 20
PY 2013
VL 773
IS 2
AR 89
DI 10.1088/0004-637X/773/2/89
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205EU
UT WOS:000323426100008
ER
PT J
AU Ackermann, M
Ajello, M
Ballet, J
Barbiellini, G
Bastieri, D
Bellazzini, R
Bonamente, E
Brandt, TJ
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Casandjian, JM
Cavazzuti, E
Cecchi, C
Chekhtman, A
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Cominsky, LR
Conrad, J
Cutini, S
Dalton, M
D'Ammando, F
de Angelis, A
Den Hartog, PR
de Palma, F
Dermer, CD
Digel, SW
Di Venere, L
Drell, PS
Dubois, R
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Franckowiak, A
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Guiriec, S
Hadasch, D
Hanabata, Y
Harding, AK
Hayashida, M
Hays, E
Hill, AB
Horan, D
Hughes, RE
Jogler, T
Johannesson, G
Johnson, AS
Johnson, TJ
Kawano, T
Kerr, M
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Latronico, L
Lemoine-Goumard, M
Li, J
Longo, F
Lovellette, MN
Lubrano, P
Mayer, M
Mazziotta, MN
McEnery, JE
Michelson, PF
Mizuno, T
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nemmen, R
Nuss, E
Ohsugi, T
Okumura, A
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Papitto, A
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Raino, S
Rando, R
Razzano, M
Rea, N
Reimer, A
Reimer, O
Scargle, JD
Schulz, A
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Takahashi, H
Thayer, JG
Thayer, JB
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Uchiyama, Y
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Werner, M
Winer, BL
Wood, KS
AF Ackermann, M.
Ajello, M.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bellazzini, R.
Bonamente, E.
Brandt, T. J.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Chekhtman, A.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Cominsky, L. R.
Conrad, J.
Cutini, S.
Dalton, M.
D'Ammando, F.
de Angelis, A.
Den Hartog, P. R.
de Palma, F.
Dermer, C. D.
Digel, S. W.
Di Venere, L.
Drell, P. S.
Dubois, R.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Franckowiak, A.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashida, M.
Hays, E.
Hill, A. B.
Horan, D.
Hughes, R. E.
Jogler, T.
Johannesson, G.
Johnson, A. S.
Johnson, T. J.
Kawano, T.
Kerr, M.
Knoedlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Latronico, L.
Lemoine-Goumard, M.
Li, J.
Longo, F.
Lovellette, M. N.
Lubrano, P.
Mayer, M.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nemmen, R.
Nuss, E.
Ohsugi, T.
Okumura, A.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Papitto, A.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Raino, S.
Rando, R.
Razzano, M.
Rea, N.
Reimer, A.
Reimer, O.
Scargle, J. D.
Schulz, A.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Takahashi, H.
Thayer, J. G.
Thayer, J. B.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Uchiyama, Y.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Werner, M.
Winer, B. L.
Wood, K. S.
TI ASSOCIATING LONG-TERM gamma-RAY VARIABILITY WITH THE SUPERORBITAL PERIOD
OF LS I+61 degrees 303
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE gamma rays: general; gamma rays: stars; stars: emission-line, Be
ID X-RAY; ORBITAL MODULATION; I +61-DEGREES-303; SPACED DATA; BINARY;
EMISSION; RADIO; STAR; OUTBURSTS; DISK
AB Gamma-ray binaries are stellar systems for which the spectral energy distribution (discounting the thermal stellar emission) peaks at high energies. Detected from radio to TeV gamma rays, the gamma-ray binary LS I + 61 degrees 303 is highly variable across all frequencies. One aspect of this system's variability is the modulation of its emission with the timescale set by the similar to 26.4960 day orbital period. Here we show that, during the time of our observations, the gamma-ray emission of LS I + 61 degrees 303 also presents a sinusoidal variability consistent with the previously known superorbital period of 1667 days. This modulation is more prominently seen at orbital phases around apastron, whereas it does not introduce a visible change close to periastron. It is also found in the appearance and disappearance of variability at the orbital period in the power spectrum of the data. This behavior could be explained by a quasi-cyclical evolution of the equatorial outflow of the Be companion star, whose features influence the conditions for generating gamma rays. These findings open the possibility to use gamma-ray observations to study the outflows of massive stars in eccentric binary systems.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Latronico, L.; 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.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brandt, T. J.; Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hays, E.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Li, J.; Papitto, A.; Rea, N.; Torres, D. F.] Inst Space Sci IEEE CSIC, E-08193 Barcelona, Spain.
[Cameron, R. A.; Chiang, J.; Claus, R.; Den Hartog, P. R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Dubois, R.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kerr, M.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA.
[Cameron, R. A.; Chiang, J.; Claus, R.; Den Hartog, P. R.; Digel, S. W.; Di Venere, L.; Drell, P. S.; Dubois, R.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kerr, M.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[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-00044 Frascati, Roma, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Roma, Italy.
[Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Universe & Particules Montpellier, CNRS, IN2P3, F-34095 Montpellier, France.
[Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA.
[Conrad, J.; Larsson, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.; Larsson, S.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden.
[Dalton, M.; Lemoine-Goumard, M.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Conrad, J.; de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[Conrad, J.; de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Dermer, C. D.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Hanabata, Y.; Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Johannesson, G.] Natl Acad Sci, Washington, DC 20001 USA.
[Johnson, T. J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, F-31028 Toulouse, France.
[Knoedlseder, J.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Larsson, S.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Lemoine-Goumard, M.; Li, J.] Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. 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.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Okumura, A.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Razzano, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Razzano, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Torres, D. F.] ICREA, E-08010 Barcelona, Spain.
[Vianello, G.] CIFS, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Chekhtman, A.; Johannesson, G.] Naval Res Lab, Washington, DC 20375 USA.
RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
EM andrea.caliandro@ieec.uab.es; hadasch@ieec.uab.es; dtorres@ieec.uab.es
RI Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Di Venere,
Leonardo/C-7619-2017; Rea, Nanda/I-2853-2015; Johannesson,
Gudlaugur/O-8741-2015; Mazziotta, Mario /O-8867-2015; Gargano,
Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Rando,
Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Reimer,
Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen,
Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Moskalenko,
Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016
OI Torres, Diego/0000-0002-1522-9065; Di Venere,
Leonardo/0000-0003-0703-824X; Giordano, Francesco/0000-0002-8651-2394;
De Angelis, Alessandro/0000-0002-3288-2517; Caraveo,
Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; Rando,
Riccardo/0000-0001-6992-818X; Rea, Nanda/0000-0003-2177-6388;
Johannesson, Gudlaugur/0000-0003-1458-7036; Mazziotta, Mario
/0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto,
nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Morselli,
Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Moskalenko,
Igor/0000-0001-6141-458X;
FU NASA (United States); U.S. Department of Energy (United States);
CEA/Irfu (France); IN2P3/CNRS (France); ASI (Italy); INFN (Italy); MEXT
(Japan); KEK (Japan); JAXA (Japan); K.A. Wallenberg Foundation (Sweden);
Swedish Research Council (Sweden); National Space Board (Sweden); INAF
in Italy; CNES in France; Alexander von Humboldt Foundation.;
[AYA2012-39303]; [SGR2009-811]; [iLINK2011-0303]
FX The Fermi-LAT Collaboration acknowledges support from a number of
agencies and institutes for both development and the operation of the
LAT as well as scientific data analysis. These include NASA and the U.S.
Department of Energy (United States); 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). Additional support from INAF in Italy and CNES in
France for science analysis during the operations phase is also
gratefully acknowledged.; Additional support of this work comes from
grants AYA2012-39303, SGR2009-811, and iLINK2011-0303. D. F. T. was
additionally supported by a Friedrich Wilhelm Bessel Award of the
Alexander von Humboldt Foundation.
NR 30
TC 16
Z9 17
U1 0
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 20
PY 2013
VL 773
IS 2
AR L35
DI 10.1088/2041-8205/773/2/L35
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 198CO
UT WOS:000322899600018
ER
PT J
AU Kamenetzky, J
McCray, R
Indebetouw, R
Barlow, MJ
Matsuura, M
Baes, M
Blommaert, JADL
Bolatto, A
Decin, L
Dunne, L
Fransson, C
Glenn, J
Gomez, HL
Groenewegen, MAT
Hopwood, R
Kirshner, RP
Lakicevic, M
Marcaide, J
Marti-Vidal, I
Meixner, M
Royer, P
Soderberg, A
Sonneborn, G
Staveley-Smith, L
Swinyard, BM
Van de Steene, G
van Hoof, PAM
van Loon, JT
Yates, J
Zanardo, G
AF Kamenetzky, J.
McCray, R.
Indebetouw, R.
Barlow, M. J.
Matsuura, M.
Baes, M.
Blommaert, J. A. D. L.
Bolatto, A.
Decin, L.
Dunne, L.
Fransson, C.
Glenn, J.
Gomez, H. L.
Groenewegen, M. A. T.
Hopwood, R.
Kirshner, R. P.
Lakicevic, M.
Marcaide, J.
Marti-Vidal, I.
Meixner, M.
Royer, P.
Soderberg, A.
Sonneborn, G.
Staveley-Smith, L.
Swinyard, B. M.
Van de Steene, G.
van Hoof, P. A. M.
van Loon, J. Th.
Yates, J.
Zanardo, G.
TI CARBON MONOXIDE IN THE COLD DEBRIS OF SUPERNOVA 1987A
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: supernova remnants; supernovae: individual (SN1987A)
ID SN 1987A; 3-DIMENSIONAL STRUCTURE; EJECTA; CASSIOPEIA; SN-1987A;
REMNANT; WAVELENGTH; INSTRUMENT; FACILITY
AB We report spectroscopic and imaging observations of rotational transitions of cold CO and SiO in the ejecta of SN1987A, the first such emission detected in a supernova remnant. In addition to line luminosities for the CO J = 1-0, 2-1, 6-5, and 7-6 transitions, we present upper limits for all other transitions up to J = 13-12, collectively measured from the Atacama Large Millimeter Array, the Atacama Pathfinder EXperiment, and the Herschel Spectral and Photometric Imaging REceiver. Simple models show the lines are emitted from at least 0.01 M-circle dot of CO at a temperature >14 K, confined within at most 35% of a spherical volume expanding at similar to 2000 km s(-1). Moreover, we locate the emission within 1 '' of the central debris. These observations, along with a partial observation of SiO, confirm the presence of cold molecular gas within supernova remnants and provide insight into the physical conditions and chemical processes in the ejecta. Furthermore, we demonstrate the powerful new window into supernova ejecta offered by submillimeter observations.
C1 [Kamenetzky, J.; McCray, R.; Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Barlow, M. J.; Matsuura, M.; Swinyard, B. M.; Yates, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Baes, M.] Univ Ghent, Steward Observ, B-9000 Ghent, Belgium.
[Blommaert, J. A. D. L.; Decin, L.; Royer, P.] Katholieke Univ Leuven, Inst Sterrenkunde, B-2001 Louvain, Belgium.
[Blommaert, J. A. D. L.] Vrije Univ Brussel, Dept Phys & Astrophys, B-1050 Brussels, Belgium.
[Bolatto, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Dunne, L.] Univ Canterbury, Dept Phys & Astron, Christchurch 8410, New Zealand.
[Fransson, C.] Stockholm Univ, Oskar Klein Ctr, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden.
[Gomez, H. L.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales.
[Groenewegen, M. A. T.; Van de Steene, G.; van Hoof, P. A. M.] Royal Observ Belgium, B-1180 Brussels, Belgium.
[Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England.
[Kirshner, R. P.; Soderberg, A.] Harvard Coll Observ, Cambridge, MA 02138 USA.
[Lakicevic, M.; van Loon, J. Th.] Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
[Marcaide, J.] Univ Valencia, E-46100 Burjassot, Spain.
[Marti-Vidal, I.] Onsala Space Observ, SE-43992 Onsala, Sweden.
[Meixner, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Sonneborn, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Staveley-Smith, L.; Zanardo, G.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia.
[Staveley-Smith, L.] Univ Western Australia, ARC Ctr Excellence All Sky Astrophys CAASTRO, Crawley, WA 6009, Australia.
RP Kamenetzky, J (reprint author), Univ Colorado, Dept Astrophys & Planetary Sci, UCB 391, Boulder, CO 80309 USA.
RI Barlow, Michael/A-5638-2009; Marti-Vidal, Ivan/A-8799-2017;
Staveley-Smith, Lister/A-1683-2011;
OI Barlow, Michael/0000-0002-3875-1171; Marti-Vidal,
Ivan/0000-0003-3708-9611; Kamenetzky, Julia/0000-0001-7877-7942;
Staveley-Smith, Lister/0000-0002-8057-0294; Zanardo,
Giovanna/0000-0003-2742-771X; Baes, Maarten/0000-0002-3930-2757
FU National Science Foundation; NSF [AST-1211196]; Belgian Science Policy
office through the ESA Prodex program; ESO/Keele studentship; MICINN
[AYA2009-130360-C02-02]; Generalitat Valenciana [PROMETEO 104/2009]
FX J.K. acknowledges funding from the National Science Foundation Graduate
Research Fellowship Program. R.K.'s supernova research at Harvard is
supported by the NSF through grant AST-1211196. J. B., P. v. H., and P.
R. acknowledge support from the Belgian Science Policy office through
the ESA Prodex program. M. L. acknowledges an ESO/Keele studentship. J.
M. received partial support from grants AYA2009-130360-C02-02 of the
MICINN and PROMETEO 104/2009 of the Generalitat Valenciana. M. Meixner
acknowledges funding support from NASA Herschel Space Center, JPL
contracts #1381522 and 1381650 and NASA NAG5-12595. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
This paper makes use of the following ALMA data: ADS/JAO.
ALMA#2011.0.00273. S. ALMA is a partnership of ESO (representing its
member states), NSF (USA) and NINS (Japan), together with NRC (Canada)
and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile.
The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ.
NR 28
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U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 20
PY 2013
VL 773
IS 2
AR L34
DI 10.1088/2041-8205/773/2/L34
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 198CO
UT WOS:000322899600017
ER
PT J
AU Mahrooghy, M
Anantharaj, VG
Younan, NH
Petersen, WA
Hsu, KL
Behrangi, A
Aanstoos, J
AF Mahrooghy, Majid
Anantharaj, Valentine G.
Younan, Nicolas H.
Petersen, Walter A.
Hsu, Kuo-Lin
Behrangi, Ali
Aanstoos, James
TI Augmenting satellite precipitation estimation with lightning information
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID RAINFALL ESTIMATION; CONVECTIVE PRECIPITATION; PASSIVE MICROWAVE;
NETWORK; TRMM; SYSTEM
AB We have used lightning information to augment the precipitation estimation from remotely sensed imagery using an artificial neural network cloud classification system (PERSIANN-CCS). Co-located lightning data are used to segregate cloud patches, segmented from Geostationary Operational Environmental Satellite (GOES)-12 infrared (IR) data, into either electrified patches (ECPs) or nonelectrified patches (NECPs). A set of features is extracted separately for the ECPs and NECPs. Features for the ECPs include a new feature corresponding to the number of flashes that occur within a 15 minute window around the time of the nominal scan of the satellite IR images of the cloud patches. The cloud patches are classified and clustered using a self-organizing maps (SOM) neural network. Then, brightness temperature and rain rate (T-R) relationships are derived for different clusters. Rain rates are estimated for the cloud patches based on their representative (T-R) relationship. The equitable threat scores (ETS) of the daily and hourly precipitation estimates at a range of rain rate thresholds show that incorporating lightning information can improve categorical precipitation estimation in the winter and fall seasons. In the winter, the ETS improvement is almost 15% for the daily and 12% for the hourly rainfall estimates (at thresholds below 15 mmhour(-1)). During the same period, there is also a drop in the false alarm ratio (FAR) and a corresponding increase in the probability of detection (POD) at most threshold levels. During the summer and spring seasons, no categorical significant improvements have been noted, except for the BIAS scores for the hourly rainfall estimates at higher thresholds (above 5 mmhour(-1)) in the summer months. A quantitative evaluation in terms of the root mean squared error (RMSE) and correlation coefficient (CORR) shows that the incorporation of lightning data does improve rainfall estimation over all seasons with the most improvement (around 11-13% CORR improvement) occurring during the winter. We speculate that during the winter, more of the ice processes are packed into a thinner stratiform layer with lower cloud tops and freezing levels. Hence, more of the ice contributes to precipitation on the ground. We also expect that information from lightning, related to the ice microphysics processes, provides surrogate information about the rain rate.
C1 [Mahrooghy, Majid; Aanstoos, James] Mississippi State Univ, Geosyst Res Inst, Mississippi State, MS 39762 USA.
[Anantharaj, Valentine G.] Oak Ridge Natl Lab, Natl Ctr Computat Sci, Oak Ridge, TN 37831 USA.
[Younan, Nicolas H.] Mississippi State Univ, Dept Elect & Comp Engn, Mississippi State, MS 39762 USA.
[Petersen, Walter A.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35899 USA.
[Hsu, Kuo-Lin] Univ Calif Irvine, Ctr Hydrometeorol & Remote Sensing, Irvine, CA 92697 USA.
[Behrangi, Ali] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mahrooghy, M (reprint author), Mississippi State Univ, Geosyst Res Inst, Mississippi State, MS 39762 USA.
EM majid@gri.msstate.edu
FU NASA Applied Sciences Program [NNS06AA98B]; NOAA Office of Atmospheric
Research [NA07OAR4170517]; Oak Ridge Leadership Computing Facility under
Office of Advanced Scientific Computing Research, Office of Science, US
Department of Energy [DE-AC05-00OR22725]; UT-Battelle, LLC.
FX This research was sponsored by the NASA Applied Sciences Program under
Grant NNS06AA98B and the NOAA Office of Atmospheric Research via Grant
NA07OAR4170517. We also thank the PERSIANN group at UC Irvine for the
PERSIANN-CCS data and the helpful discussions about their methodology.
Valentine Anantharaj is also supported by the Oak Ridge Leadership
Computing Facility under the auspices of the Office of Advanced
Scientific Computing Research, Office of Science, US Department of
Energy under Contract No. DE-AC05-00OR22725 and Contract No.
DE-AC05-00OR22725 with UT-Battelle, LLC.
NR 33
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U1 0
U2 16
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0143-1161
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PD AUG 20
PY 2013
VL 34
IS 16
BP 5796
EP 5811
DI 10.1080/01431161.2013.796100
PG 16
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA 161IZ
UT WOS:000320187700010
ER
PT J
AU Shuai, YM
Schaaf, C
Zhang, XY
Strahler, A
Roy, D
Morisette, J
Wang, ZS
Nightingale, J
Nickeson, J
Richardson, AD
Xie, DH
Wang, JD
Li, XW
Strabala, K
Davies, JE
AF Shuai, Yanmin
Schaaf, Crystal
Zhang, Xiaoyang
Strahler, Alan
Roy, David
Morisette, Jeffrey
Wang, Zhuosen
Nightingale, Joanne
Nickeson, Jaime
Richardson, Andrew D.
Xie, Donghui
Wang, Jindi
Li, Xiaowen
Strabala, Kathleen
Davies, James E.
TI Daily MODIS 500 m reflectance anisotropy direct broadcast (DB) products
for monitoring vegetation phenology dynamics
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID DECIDUOUS BROADLEAF FOREST; IMAGING SPECTRORADIOMETER MODIS;
LAND-SURFACE PHENOLOGY; SPRING PHENOLOGY; CLIMATE-CHANGE; GLOBAL CHANGE;
NEAR-SURFACE; RAINY-SEASON; REAL-TIME; VARIABILITY
AB Land surface vegetation phenology is an efficient bio-indicator for monitoring ecosystem variation in response to changes in climatic factors. The primary objective of the current article is to examine the utility of the daily MODIS 500 m reflectance anisotropy direct broadcast (DB) product for monitoring the evolution of vegetation phenological trends over selected crop, orchard, and forest regions. Although numerous model-fitted satellite data have been widely used to assess the spatio-temporal distribution of land surface phenological patterns to understand phenological process and phenomena, current efforts to investigate the details of phenological trends, especially for natural phenological variations that occur on short time scales, are less well served by remote sensing challenges and lack of anisotropy correction in satellite data sources. The daily MODIS 500 m reflectance anisotropy product is employed to retrieve daily vegetation indices (VI) of a 1 year period for an almond orchard in California and for a winter wheat field in northeast China, as well as a 2 year period for a deciduous forest region in New Hampshire, USA. Compared with the ground records from these regions, the VI trajectories derived from the cloud-free and atmospherically corrected MODIS Nadir BRDF (bidirectional reflectance distribution function) adjusted reflectance (NBAR) capture not only the detailed footprint and principal attributes of the phenological events (such as flowering and blooming) but also the substantial inter-annual variability. This study demonstrates the utility of the daily 500 m MODIS reflectance anisotropy DB product to provide daily VI for monitoring and detecting changes of the natural vegetation phenology as exemplified by study regions comprising winter wheat, almond trees, and deciduous forest.
C1 [Shuai, Yanmin] NASA, ERT Inc, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Schaaf, Crystal; Wang, Zhuosen] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA.
[Zhang, Xiaoyang] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Zhang, Xiaoyang] NOAA, NESDIS, STAR, College Pk, MD USA.
[Strahler, Alan] Boston Univ, Dept Earth & Environm, Ctr Remote Sensing, Boston, MA 02215 USA.
[Roy, David] S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA.
[Morisette, Jeffrey] US Geol Survey, DOI North Cent Climate Sci Ctr, Ft Collins, CO 80525 USA.
[Nightingale, Joanne; Nickeson, Jaime] NASA, Sigma Space Corp, Terr Informat Syst Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Richardson, Andrew D.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Xie, Donghui; Wang, Jindi; Li, Xiaowen] Beijing Normal Univ, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China.
[Xie, Donghui; Wang, Jindi; Li, Xiaowen] Chinese Acad Sci, Inst Remote Sensing Applicat, Beijing, Peoples R China.
[Xie, Donghui; Wang, Jindi; Li, Xiaowen] Beijing Normal Univ, Beijing Key Lab Remote Sensing Environm & Digital, Beijing 100875, Peoples R China.
[Xie, Donghui; Wang, Jindi; Li, Xiaowen] Beijing Normal Univ, Sch Geog & Remote Sensing Sci, Beijing 100875, Peoples R China.
[Strabala, Kathleen; Davies, James E.] UW Madison, SSEC, Madison, WI 53706 USA.
RP Shuai, YM (reprint author), NASA, ERT Inc, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Yanmin.Shuai@nasa.gov
RI Zhang, Xiaoyang/E-3208-2010; Richardson, Andrew/F-5691-2011
OI Richardson, Andrew/0000-0002-0148-6714
FU NASA [NNX08AE94A]; State Key Laboratory of Remote Sensing Science
[OFSLRSS201102]; National Science Foundation, through the Macrosystems
Biology programme [EF-1065029]; Northeastern States Research
Cooperative; US Geological Survey Status and Trends Program; US National
Park Service Inventory and Monitoring Program; USA National Phenology
Network through US Geological Survey [G10AP00129]
FX This work was supported by NASA NNX08AE94A. The authors would like to
thank researchers at the YCES (Yucheng Experiment Station, Chinese
Academic Sciences (CAS)), contributors to the blue diamond website
(http://www.bluediamond.com/applications/in-the-field), contributors to
the foliage network (http://www.foliagenetwork.net), researchers at the
Bartlett Experiment Forest site for providing the ground phenology
information, and a thorough and thoughtful review of the manuscript by
Jesslyn Brown, US Geological Survey. Dr Donghui Xie acknowledges support
from the open funding programme of the State Key Laboratory of Remote
Sensing Science (#OFSLRSS201102). Dr Andrew D. Richardson acknowledges
support from the National Science Foundation, through the Macrosystems
Biology programme, award EF-1065029; the Northeastern States Research
Cooperative; and the US Geological Survey Status and Trends Program, the
US National Park Service Inventory and Monitoring Program, and the USA
National Phenology Network through grant number G10AP00129 from the US
Geological Survey. Any use of trade, product, or firm names is for
descriptive purposes only and does not imply endorsement by the US
Government.
NR 70
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Z9 15
U1 1
U2 63
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0143-1161
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PD AUG 20
PY 2013
VL 34
IS 16
BP 5997
EP 6016
DI 10.1080/01431161.2013.803169
PG 20
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA 161IZ
UT WOS:000320187700021
ER
PT J
AU Corley, AM
White, H
AF Corley, Anne-Marie
White, Harold 'Sonny'
TI One minute with ... Harold 'Sonny' White
SO NEW SCIENTIST
LA English
DT Editorial Material
C1 [White, Harold 'Sonny'] NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 1
U2 5
PU REED BUSINESS INFORMATION LTD
PI SUTTON
PA QUADRANT HOUSE THE QUADRANT, SUTTON SM2 5AS, SURREY, ENGLAND
SN 0262-4079
J9 NEW SCI
JI New Sci.
PD AUG 17
PY 2013
VL 219
IS 2930
BP 27
EP 27
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 203NR
UT WOS:000323300400018
ER
PT J
AU Li, JLF
Waliser, DE
Stephens, G
Lee, S
L'Ecuyer, T
Kato, S
Loeb, N
Ma, HY
AF Li, J. -L. F.
Waliser, D. E.
Stephens, G.
Lee, Seungwon
L'Ecuyer, T.
Kato, Seiji
Loeb, Norman
Ma, Hsi-Yen
TI Characterizing and understanding radiation budget biases in CMIP3/CMIP5
GCMs, contemporary GCM, and reanalysis
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Radiation; CMIP3; CMIP5
ID SATELLITE-OBSERVATIONS; ATMOSPHERE RADIATION; TRANSFER MODEL; ISCCP
DATA; DATA SETS; IN-SITU; CLOUD; SURFACE; TOP; ECMWF
AB We evaluate the annual mean radiative shortwave flux downward at the surface (RSDS) and reflected shortwave (RSUT) and radiative longwave flux upward at top of atmosphere (RLUT) from the twentieth century Coupled Model Intercomparison Project Phase 5 (CMIP5) and Phase 3 (CMIP3) simulations as well as from the NASA GEOS5 model and Modern-Era Retrospective Analysis for Research and Applications analysis. The results show that a majority of the models have significant regional biases in the annual means of RSDS, RLUT, and RSUT, with biases from -30 to 30Wm(-2). While the global average CMIP5 ensemble mean biases of RSDS, RLUT, and RSUT are reduced compared to CMIP3 by about 32% (e.g., -6.9 to 2.5Wm(-2)), 43%, and 56%, respectively. This reduction arises from a more complete cancellation of the pervasive negative biases over ocean and newly larger positive biases over land. In fact, based on these biases in the annual mean, Taylor diagram metrics, and RMSE, there is virtually no progress in the simulation fidelity of RSDS, RLUT, and RSUT fluxes from CMIP3 to CMIP5. A persistent systematic bias in CMIP3 and CMIP5 is the underestimation of RSUT and overestimation of RSDS and RLUT in the convectively active regions of the tropics. The amount of total ice and liquid atmospheric water content in these areas is also underestimated. We hypothesize that at least a part of these persistent biases stem from the common global climate model practice of ignoring the effects of precipitating and/or convective core ice and liquid in their radiation calculations.
C1 [Li, J. -L. F.; Waliser, D. E.; Stephens, G.; Lee, Seungwon] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[L'Ecuyer, T.] Univ Wisconsin Madison, Madison, WI USA.
[Kato, Seiji; Loeb, Norman] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Ma, Hsi-Yen] Lawrence Livermore Natl Lab, Livermore, CA USA.
RP Li, JLF (reprint author), CALTECH, Jet Prop Lab, NASA, MS 233-306K,4800 Ak Grove Dr, Pasadena, CA 91109 USA.
EM Juilin.F.Li@jpl.nasa.gov
RI Ma, Hsi-Yen/K-1019-2013; L'Ecuyer, Tristan/E-5607-2012
OI L'Ecuyer, Tristan/0000-0002-7584-4836
FU U.S. Department of Energy by Lawrence Livermore National Laboratory
[DE-AC52-07NA27344]
FX We would like to thank the Editor and two reviewers for giving very
insightful and helpful comments and suggestions. We thank Prof. M-D
Chou/NCU and Dr. W-L Lee/RCEC-Academia Sinica for useful comments; Dr.
Anthony Del Genio/NASA GISS, Dr. Ken Lo/NASA GISS, Dr. Voldoir
Aurore/CNRM, Dr. Masahiro Watanabe and Dr. Shingo Watanabe/MIROC, Dr.
Leon Rotstayn/CSIRO, Dr. Knut von Salzen/CCCma, Dr. Gary Strand/NCAR,
Dr. Alf Kirkevag/NCC, Dr. Seiji Yukimoto/MRI, Dufresne Jean-Louis/IPSL,
Dr. Tongwen Wu/BCC-CMA, and many other colleagues from climate modeling
centers for providing model information. Thanks also to Prof. W-T Anne
Chen/NTU when at JPL and Gregory Huey/JPL with data. The contributions
by DEW and JLL to this study were carried out on behalf of the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. The
contribution of Hsi-Yen Ma to this work was performed under the auspices
of the U.S. Department of Energy by Lawrence Livermore National
Laboratory under contract DE-AC52-07NA27344.
NR 65
TC 39
Z9 41
U1 0
U2 20
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 AUG 16
PY 2013
VL 118
IS 15
BP 8166
EP 8184
DI 10.1002/jgrd.50378
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 213DA
UT WOS:000324032900004
ER
PT J
AU Hill, JD
Pilkey, J
Uman, MA
Jordan, DM
Rison, W
Krebhiel, PR
Biggerstaff, MI
Hyland, P
Blakeslee, R
AF Hill, J. D.
Pilkey, J.
Uman, M. A.
Jordan, D. M.
Rison, W.
Krebhiel, P. R.
Biggerstaff, M. I.
Hyland, P.
Blakeslee, R.
TI Correlated lightning mapping array and radar observations of the initial
stages of three sequentially triggered Florida lightning discharges
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE lightning
ID THUNDERSTORM; EVOLUTION; SIGNATURES; WSR-88D; SYSTEM
AB Correlated Lightning Mapping Array and vertical-scan radar images are presented for three rocket-and-wire triggered lightning flashes that occurred sequentially within 17min in the presence of a decaying multicellular convective storm system over north-central Florida. The initial stage (IS) of each flash propagated generally vertically to the altitude of the 0 degrees C melting level, about 5km, and then subsequently propagated for many kilometers horizontally along the melting level contour. Radar images suggest that the propagation paths of the IS channels below and above the melting level were heavily influenced by precipitation gradients. Flash UF 11-24 exhibited a 12.6km unbranched IS channel, the longest unbranched channel observed in the study by a factor of three. During flash UF 11-25 (119ms following the cessation of the measured IS current at ground and prior to the first return stroke), a natural cloud-to-ground discharge, perhaps induced by the IS, initiated between 2.5 and 4km altitude and struck ground 5 to 7km from the launching facility. The IS of flash UF 11-26 propagated upward through a descending precipitation packet and apparently induced a naturally appearing bi-level intracloud discharge via an upward-negative leader that initiated within the IS breakdown region 3.5km from the launching facility. The upward-negative leader propagated from 5.6 to 9.3km altitude in a time of 11ms. The electrical current measured at ground during the IS of flash UF 11-26 exhibited a 57ms polarity reversal, transferring 19 C of positive charge to ground.
C1 [Hill, J. D.; Pilkey, J.; Uman, M. A.; Jordan, D. M.] Univ Florida, Dept Elect & Comp Engn, Gainesville, FL 32611 USA.
[Rison, W.; Krebhiel, P. R.] New Mexico Inst Min & Technol, Dept Elect Engn, Dept Phys, Socorro, NM 87801 USA.
[Biggerstaff, M. I.; Hyland, P.] Univ Oklahoma, Sch Meteorol, Norman, OK 73019 USA.
[Blakeslee, R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Hill, JD (reprint author), Univ Florida, Dept Elect & Comp Engn, POB 116200,311 Larsen Hall, Gainesville, FL 32611 USA.
EM jonathan.d.hill@nasa.gov
OI Biggerstaff, Michael/0000-0002-6690-784X
FU DARPA NIMBUS program; NASA; National Science Foundation [AGS-1063537]
FX This research was primarily funded by the DARPA NIMBUS program with
additional support from NASA. M. Biggerstaff was partially supported by
National Science Foundation grant AGS-1063537. The authors would also
like to thank G. Carrie, K. Thiem, T. Ngin, W. Gamerota, N. Brooks, A.
Dunhoft, and J. Jordan for their assistance in the data collection
effort.
NR 43
TC 9
Z9 9
U1 1
U2 16
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 AUG 16
PY 2013
VL 118
IS 15
BP 8460
EP 8481
DI 10.1002/jgrd.50660
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 213DA
UT WOS:000324032900025
ER
PT J
AU Yue, Q
Kahn, BH
Xiao, H
Schreier, MM
Fetzer, EJ
Teixeira, J
Suselj, K
AF Yue, Qing
Kahn, Brian H.
Xiao, Heng
Schreier, Mathias M.
Fetzer, Eric J.
Teixeira, Joao
Suselj, Kay
TI Transitions of cloud-topped marine boundary layers characterized by
AIRS, MODIS, and a large eddy simulation model
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Marine boundary layer cloud; transition; collocated satellite
observation; Large eddy simulation
ID LIQUID WATER PATH; SHALLOW CUMULUS CONVECTION; ENTRAINMENT INSTABILITY;
STRATOCUMULUS CLOUDS; MIXED LAYERS; TEMPERATURE-MEASUREMENTS; RADIATIVE
PROPERTIES; PRECIPITABLE WATER; STRONG INVERSION; SATELLITE
AB Cloud top entrainment instability (CTEI) is a hypothesized positive feedback between entrainment mixing and evaporative cooling near the cloud top. Previous theoretical and numerical modeling studies have shown that the persistence or breakup of marine boundary layer (MBL) clouds may be sensitive to the CTEI parameter. Collocated thermodynamic profile and cloud observations obtained from the Atmospheric Infrared Sounder (AIRS) and Moderate Resolution Imaging Spectroradiometer (MODIS) instruments are used to quantify the relationship between the CTEI parameter and the cloud-topped MBL transition from stratocumulus to trade cumulus in the northeastern Pacific Ocean. Results derived from AIRS and MODIS are compared with numerical results from the UCLA large eddy simulation (LES) model for both well-mixed and decoupled MBLs. The satellite and model results both demonstrate a clear correlation between the CTEI parameter and MBL cloud fraction. Despite fundamental differences between LES steady state results and the instantaneous snapshot type of observations from satellites, significant correlations for both the instantaneous pixel-scale observations and the long-term averaged spatial patterns between the CTEI parameter and MBL cloud fraction are found from the satellite observations and are consistent with LES results. This suggests the potential of using AIRS and MODIS to quantify global and temporal characteristics of the cloud-topped MBL transition.
C1 [Yue, Qing; Kahn, Brian H.; Schreier, Mathias M.; Fetzer, Eric J.; Teixeira, Joao; Suselj, Kay] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Yue, Qing; Schreier, Mathias M.; Suselj, Kay] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Xiao, Heng] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
RP Yue, Q (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
EM Qing.Yue@jpl.nasa.gov
RI Yue, Qing/F-4619-2017
OI Yue, Qing/0000-0002-3559-6508
FU NASA; Office of Naval Research [N0001411IP20087, N0001411IP20069]; NASA
MAP Program; NOAA/CPO MAPP Program; NOAA at UCLA [NA07OAR4310236]; U.S.
DOE OBER grant at PNNL [KP/501021/58166]; Battelle Memorial Institute
[DE-AC05-76RL01830]; AIRS Project at JPL
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. Q.Y.
and E.J.F. were supported by NASA's Making Earth Science Data Records
for Use in Research Environments (MEaSUREs) program. J.T. and K. S.
acknowledge the support provided by the Office of Naval Research, Marine
Meteorology Program under Awards N0001411IP20087 and N0001411IP20069,
the NASA MAP Program, and the NOAA/CPO MAPP Program. Funding for H. X.
is provided by NOAA Grant NA07OAR4310236 at UCLA and by U.S. DOE OBER
grant KP/501021/58166 at PNNL. The Pacific Northwest National Laboratory
is operated for DOE by Battelle Memorial Institute under Contract No.
DE-AC05-76RL01830. Q.Y., E.J.F., J.T., M. M. S., and B. H. K.
acknowledge the support of the AIRS Project at JPL. 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 would like to
thank Jui-Lin Li and Terry Kubar for useful feedback in the preparation
of this manuscript.
NR 80
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Z9 5
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 16
PY 2013
VL 118
IS 15
BP 8598
EP 8611
DI 10.1002/jgrd.50676
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 213DA
UT WOS:000324032900033
ER
PT J
AU Li, J
Carlson, BE
Lacis, AA
AF Li, Jing
Carlson, Barbara E.
Lacis, Andrew A.
TI Application of spectral analysis techniques in the intercomparison of
aerosol data: 1. An EOF approach to analyze the spatial-temporal
variability of aerosol optical depth using multiple remote sensing data
sets
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE aerosol; spatial-temporal variability; multi-sensor; EOF analysis
ID RETRIEVALS; LAND; OCEAN
AB Many remote sensing techniques and passive sensors have been developed to measure global aerosol properties. While instantaneous comparisons between pixel-level data often reveal quantitative differences, here we use Empirical Orthogonal Function (EOF) analysis, also known as Principal Component Analysis, to demonstrate that satellite-derived aerosol optical depth (AOD) data sets exhibit essentially the same spatial and temporal variability and are thus suitable for large-scale studies. Analysis results show that the first four EOF modes of AOD account for the bulk of the variance and agree well across the four data sets used in this study (i.e., Aqua MODIS, Terra MODIS, MISR, and SeaWiFS). Only SeaWiFS data over land have slightly different EOF patterns. Globally, the first two EOF modes show annual cycles and are mainly related to Sahara dust in the northern hemisphere and biomass burning in the southern hemisphere, respectively. After removing the mean seasonal cycle from the data, major aerosol sources, including biomass burning in South America and dust in West Africa, are revealed in the dominant modes due to the different interannual variability of aerosol emissions. The enhancement of biomass burning associated with El Nino over Indonesia and central South America is also captured with the EOF technique.
C1 [Li, Jing; Carlson, Barbara E.; Lacis, Andrew A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Li, Jing] Oak Ridge Associated Univ, NASA, Postdoctoral Fellowship Program, Oak Ridge, TN USA.
RP Li, J (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM Jing.Li@nasa.gov
FU climate grant [509496.02.08.04.24]; NASA Postdoctoral Program (NPP)
FX We thank the MODIS, MISR, and SeaWiFS science teams for providing the
data used in this study. We also thank the anonymous reviewers for
providing many helpful comments and suggestions. This study is funded by
climate grant 509496.02.08.04.24. Jing Li is also funded by the NASA
Postdoctoral Program (NPP).
NR 23
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U1 3
U2 22
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 16
PY 2013
VL 118
IS 15
BP 8640
EP 8648
DI 10.1002/jgrd.50686
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 213DA
UT WOS:000324032900036
ER
PT J
AU Ashour-Abdalla, M
Schriver, D
Alaoui, M
Richard, R
Walker, R
Goldstein, ML
Donovan, E
Zhou, M
AF Ashour-Abdalla, Maha
Schriver, David
El Alaoui, Mostafa
Richard, Robert
Walker, Raymond
Goldstein, Melvyn L.
Donovan, Eric
Zhou, Meng
TI Direct auroral precipitation from the magnetotail during substorms
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Acceleration; Dipolarization; Auroral; magnetotail; substorm
ID ELECTRIC-FIELDS; PLASMA SHEET; ACCELERATION; SIMULATIONS; PARTICLES;
BURSTS; ARRAY
AB In this study, we examine the causes of electron precipitation during a substorm on 15 February 2008 that lead to auroral brightening. We use global kinetic simulations along with spacecraft and ground-based data. We find similar to keV electrons in the region modeled in the simulation precipitate into the premidnight sector at latitudes between 71 degrees and 75 degrees due to two distinct physical processes: (1) higher latitude precipitation due to electrons that undergo relatively rapid non-adiabatic pitch angle scattering into the loss cone just earthward of a reconnection region, and (2) lower latitude precipitation due to electrons that are more gradually accelerated primarily parallel to the geomagnetic field by Fermi acceleration. These latter electrons enter the loss cone much closer to Earth at similar to-15 to -10 R-E. The electron precipitation due to the combination of these two mechanisms coincides spatially with observed auroral brightening during the disturbed event.
C1 [Ashour-Abdalla, Maha; Schriver, David; El Alaoui, Mostafa; Richard, Robert; Walker, Raymond] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Ashour-Abdalla, Maha; Schriver, David; El Alaoui, Mostafa; Richard, Robert] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Walker, Raymond] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Walker, Raymond] Natl Sci Fdn, Arlington, VA 22230 USA.
[Goldstein, Melvyn L.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA.
[Donovan, Eric] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Zhou, Meng] Nanchang Univ, Inst Space Sci & Technol, Nanchang, Peoples R China.
RP Ashour-Abdalla, M (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, 405 Hilgard Ave,3860 Slichter Hall, Los Angeles, CA 90095 USA.
EM mabdalla@igpp.ucla.edu
OI Donovan, Eric/0000-0002-8557-4155
FU NASA MMS Interdisciplinary Science Program [NNX08AO48G]; NASA
[NNX12AD13G, NASA-GI NX10AQ47G, NAS5-02099]; NSF GEM [AGS-1203739]; NSF
[AGS-1241405]; NSF Independent Research and Development program; MMS IDS
program at Goddard Space Flight Center
FX Research at UCLA was supported by the NASA MMS Interdisciplinary Science
Program grant NNX08AO48G, NASA grant NNX12AD13G, NASA-GI NX10AQ47G, NSF
GEM grant AGS-1203739 and NSF AGS-1241405. RJW was on leave at NSF and
this work was supported by the NSF Independent Research and Development
program. MLG was supported in part by the MMS IDS program at Goddard
Space Flight Center. We acknowledge NASA contract NAS5-02099 and V.
Angelopoulos for use of data from the THEMIS Mission. Computing was
carried out on NASA Advanced Supercomputing and NSF XSEDE platforms.
NR 30
TC 4
Z9 4
U1 0
U2 19
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2013
VL 40
IS 15
BP 3787
EP 3792
DI 10.1002/grl.50635
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 208EO
UT WOS:000323660000001
ER
PT J
AU Young, KE
van Soest, MC
Hodges, KV
Watson, EB
Adams, BA
Lee, P
AF Young, Kelsey E.
van Soest, Matthijs C.
Hodges, Kip V.
Watson, E. Bruce
Adams, Byron A.
Lee, Pascal
TI Impact thermochronology and the age of Haughton impact structure, Canada
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Haughton crater; (U-Th); He thermochronology; impact dating
ID LASER PROBE AR-40/AR-39; DEVON-ISLAND; SHOCK METAMORPHISM; TEMPERATURE;
ASTROBLEME; DIFFUSION
AB Most successful efforts to determine the ages of impact events are based on the isotope geochronology of crystalline or glassy impact melts. Studies of impact sites on Earth show that many form without significant melt production, meaning that traditional geochronologic approaches can yield unsatisfying results. We describe here an alternative approach based on theoretical calculations that even brief thermal events related to impact can reset the isotopic systematics of unmelted target rocks. Thermochronometers based on the production of radiogenic He-4 in accessory minerals are particularly amenable to complete resetting by impact and should yield robust impact ages if helium systematics are not further disturbed during post-impact thermal events. We illustrate the utility of this method through a presentation of a new zircon (U-Th)/He date for the Haughton impact structure, Canada, of 23.5 +/- 2.0Ma.
C1 [Young, Kelsey E.; van Soest, Matthijs C.; Hodges, Kip V.; Adams, Byron A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Watson, E. Bruce] Rensselaer Polytech Inst, Dept Earth & Environm Sci, Troy, NY USA.
[Lee, Pascal] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Young, KE (reprint author), Arizona State Univ, Sch Earth & Space Explorat, POB 876004, Tempe, AZ 85287 USA.
EM keyoung4@asu.edu
RI Hodges, Kip/A-7992-2009; Adams, Byron/I-4243-2015
OI Hodges, Kip/0000-0003-2805-8899; Adams, Byron/0000-0001-8219-3544
FU NASA [NNX09AW29G, NNX11AB31G, NNX10AK72H]
FX We would like to thank John Schutt, Jesse Weaver, Travis Oaks, and all
those involved in the 2010 Haughton Mars Project for their logistical
support in the field. We acknowledge the NASA Ames Research Center's
Intelligent Robotics Group and thank them for the field and travel
support. Alka Tripathy and Cameron Mercer are acknowledged for their
help in laboratory analysis. We would also like to thank NASA for
funding travel to Haughton (grant #NNX09AW29G), providing analytical
funds (grant #NNX11AB31G), and granting additional funding for K.E.Y.
(grant #NNX10AK72H). We also thank Kyle Min and Tom Shoberg for their
thoughtful reviews.
NR 30
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Z9 7
U1 1
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2013
VL 40
IS 15
BP 3836
EP 3840
DI 10.1002/grl.50745
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 208EO
UT WOS:000323660000010
ER
PT J
AU Bryant, AC
Painter, TH
Deems, JS
Bender, SM
AF Bryant, Ann C.
Painter, Thomas H.
Deems, Jeffrey S.
Bender, Stacie M.
TI Impact of dust radiative forcing in snow on accuracy of operational
runoff prediction in the Upper Colorado River Basin
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE dust; radiative forcing; streamflow; snow hydrology; MODIS
ID ENERGY-BALANCE; CLIMATE; DEPOSITION; ALBEDO; REGION; MODEL
AB Accurate prediction of snowmelt runoff is critical in the US Intermountain West, where water demand is increasing and snow patterns are shifting. Here, we show that errors in the National Weather Service Colorado Basin River Forecast Center's operational streamflow predictions are correlated with the interannual variability of dust radiative forcing in snow. With data from 2000-2010, we show that errors in snowmelt period streamflow prediction for the southern Colorado Rockies are linearly related to melt period dust radiative forcing in snow as inferred from NASA Moderate Resolution Imaging Spectroradiometer data, which ranged interannually from 20 to 80 W m(-2). Each 10 W m(-2) change of melt period dust forcing resulted in a corresponding change in runoff prediction bias of 10.0% +/- 1.5% and a 1.5 +/- 0.6 day shift in runoff center of mass. Accounting for bias introduced by dust forcing could improve streamflow prediction in regions prone to dust deposition in the snowpack.
C1 [Bryant, Ann C.] Univ Utah, Dept Geog, Salt Lake City, UT 84112 USA.
[Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Deems, Jeffrey S.] Natl Snow & Ice Data Ctr, Boulder, CO USA.
[Deems, Jeffrey S.] NOAA Western Water Assessment, Boulder, CO USA.
[Bender, Stacie M.] NOAA, Natl Weather Serv, Colorado Basin River Forecast Ctr, Salt Lake City, UT USA.
RP Bryant, AC (reprint author), Univ Utah, Dept Geog, 260 S Cent Campus Dr,Rm 270, Salt Lake City, UT 84112 USA.
EM anniebryant@gmail.com
RI Painter, Thomas/B-7806-2016; Deems, Jeffrey/E-6484-2016
OI Deems, Jeffrey/0000-0002-3265-8670
FU NASA [NNX10A097G, NNX09A038HS01]; NASA Applied Sciences program
FX This work was funded by NASA projects NNX10A097G and NNX09A038HS01 and
the NASA Applied Sciences program. Part of this work was performed at
the Jet Propulsion Laboratory, California Institute of Technology under
a contract with NASA.
NR 24
TC 8
Z9 8
U1 2
U2 35
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2013
VL 40
IS 15
BP 3945
EP 3949
DI 10.1002/grl.50773
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 208EO
UT WOS:000323660000031
ER
PT J
AU Ham, YG
Kug, JS
Park, JY
AF Ham, Yoo-Geun
Kug, Jong-Seong
Park, Jong-Yeon
TI Two distinct roles of Atlantic SSTs in ENSO variability: North Tropical
Atlantic SST and Atlantic Nino
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Atlantic SST; ENSO
ID TONGUE EL-NINO; INDIAN-OCEAN; WARM POOL; INTERACTIVE FEEDBACK; EVENTS;
RAINFALL; MODEL
AB Two distinct roles of the Atlantic sea surface temperatures (SSTs), namely, the North Tropical Atlantic (NTA) SST and the Atlantic Nino, on the El Nino-Southern Oscillation (ENSO) variability are investigated using the observational data from 1980 to 2010 and coupled model experiments. It appears that the NTA SST and the Atlantic Nino can be used as two independent predictors for predicting the development of ENSO events in the following season. Furthermore, they are likely to be linked to different types of El Nino events. Specifically, the NTA SST cooling during February, March, and April contributes to the central Pacific warming at the subsequent winter season, while the negative Atlantic Nino event during June, July, and August contributes to enhancing the eastern Pacific warming. The coupled model experiments support these results. With the aid of a lagged inverse relationship, the statistical forecast using two Atlantic indices can successfully predict various ENSO indices.
C1 [Ham, Yoo-Geun] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Ham, Yoo-Geun] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA.
[Kug, Jong-Seong] Korea Inst Ocean Sci & Technol, Ansan, South Korea.
[Park, Jong-Yeon] Max Planck Inst Meteorol, D-20146 Hamburg, Germany.
RP Kug, JS (reprint author), Korea Inst Ocean Sci & Technol, Ansan, South Korea.
EM jskug@kiost.ac
RI KUG, JONG-SEONG/A-8053-2013
FU Korea Meteorological Administration Research and Development Program
[CATER 2012-3042]; KIOST [PE99162]; Korea Institute of Science and
Technology Information [KSC-2012-C2-25]
FX This work was funded by the Korea Meteorological Administration Research
and Development Program under grant CATER 2012-3042 and KIOST (PE99162).
The modeling integration was supported by grant KSC-2012-C2-25 from
Korea Institute of Science and Technology Information.
NR 31
TC 15
Z9 16
U1 1
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2013
VL 40
IS 15
BP 4012
EP 4017
DI 10.1002/grl.50729
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 208EO
UT WOS:000323660000043
ER
PT J
AU Garfinkel, CI
Hurwitz, MM
Oman, LD
Waugh, DW
AF Garfinkel, Chaim I.
Hurwitz, Margaret M.
Oman, Luke D.
Waugh, Darryn W.
TI Contrasting Effects of Central Pacific and Eastern Pacific El Nino on
stratospheric water vapor
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ENSO; stratospheric water vapor; Central Pacific El Nino; tropical
tropopause layer; chemistry-climate model
ID TROPICAL TROPOPAUSE; TEMPERATURE; ENSO; VARIABILITY; CLIMATE; EVENTS;
LAYER
AB Targeted experiments with a comprehensive chemistry-climate model are used to demonstrate that seasonality and the location of the peak warming of sea surface temperatures dictate the response of stratospheric water vapor to El Nino. In boreal spring, El Nino events in which sea surface temperature anomalies peak in the eastern Pacific lead to a warming at the tropopause above the warm pool region, and subsequently to more stratospheric water vapor (consistent with previous work). However, in fall and in early winter, and also during El Nino events in which the sea surface temperature anomaly is found mainly in the central Pacific, the response is qualitatively different: temperature changes in the warm pool region and specifically over the cold point region are nonuniform, and less water vapor enters the stratosphere. The difference in water vapor in the lower stratosphere between the two variants of El Nino approaches 0.3ppmv, while the difference between the winter and spring responses exceeds 0.5ppmv.
C1 [Garfinkel, Chaim I.; Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Hurwitz, Margaret M.] Morgan State Univ, NASA GESTAR, Greenbelt, MD USA.
[Hurwitz, Margaret M.; Oman, Luke D.] NASA GSFC, Greenbelt, MD USA.
RP Garfinkel, CI (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
EM cig4@jhu.edu
RI Oman, Luke/C-2778-2009; garfinkel, chaim/H-6215-2012; Waugh,
Darryn/K-3688-2016
OI Oman, Luke/0000-0002-5487-2598; garfinkel, chaim/0000-0001-7258-666X;
Waugh, Darryn/0000-0001-7692-2798
FU NSF [AGS-1036858, ATM-0905863]
FX This work was supported by NSF grants AGS-1036858 and ATM-0905863.
NR 36
TC 3
Z9 3
U1 1
U2 18
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 AUG 16
PY 2013
VL 40
IS 15
BP 4115
EP 4120
DI 10.1002/grl.50677
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 208EO
UT WOS:000323660000061
ER
PT J
AU Meromy, L
Molotch, NP
Link, TE
Fassnacht, SR
Rice, R
AF Meromy, Leah
Molotch, Noah P.
Link, Timothy E.
Fassnacht, Steven R.
Rice, Robert
TI Subgrid variability of snow water equivalent at operational snow
stations in the western USA
SO HYDROLOGICAL PROCESSES
LA English
DT Article
DE snow; modelling; snow water equivalent; water resources; SNOTEL
ID SPATIAL-DISTRIBUTION; ENERGY-BALANCE; ALPINE BASIN; COVER; FOREST;
MODEL; ACCUMULATION; POINT; SCALE; INTERPOLATION
AB The spatial distribution of snow water equivalent (SWE) is a key variable in many regional-scale land surface models. Currently, the assimilation of point-scale snow sensor data into these models is commonly performed without consideration of the spatial representativeness of the point data with respect to the model grid-scale SWE. To improve the understanding of the relationship between point-scale snow measurements and surrounding areas, we characterized the spatial distribution of snow depth and SWE within 1-, 4- and 16-km(2) grids surrounding 15 snow stations (snowpack telemetry and California snow sensors) in California, Colorado, Wyoming, Idaho and Oregon during the 2008 and 2009 snow seasons. More than 30000 field observations of snowpack properties were used with binary regression tree models to relate SWE at the sensor site to the surrounding area SWE to evaluate the sensor representativeness of larger-scale conditions. Unlike previous research, we did not find consistent high biases in snow sensor depth values as biases over all sites ranged from 74% overestimates to 77% underestimates. Of the 53 assessments, 27 surveys indicated snow station biases of less than 10% of the surrounding mean observed snow depth. Depth biases were largely dictated by the physiographic relationship between the snow sensor locations and the mean characteristics of the surrounding grid, in particular, elevation, solar radiation index and vegetation density. These scaling relationships may improve snow sensor data assimilation; an example application is illustrated for the National Operational Hydrologic Remote Sensing Center National Snow Analysis SWE product. The snow sensor bias information indicated that the assimilation of point data into the National Operational Hydrologic Remote Sensing Center model was often unnecessary and reduced model accuracy. Copyright (c) 2012 John Wiley & Sons, Ltd.
C1 [Meromy, Leah; Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Dept Geog, Boulder, CO 80309 USA.
[Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Link, Timothy E.] Univ Idaho, Dept Forest Ecol & Biogeosci, Moscow, ID 83843 USA.
[Fassnacht, Steven R.] Colorado State Univ, ESS Watershed Sci, Ft Collins, CO 80523 USA.
[Rice, Robert] Univ Calif Merced, Sierra Nevada Res Inst, Merced, CA USA.
RP Meromy, L (reprint author), Univ Colorado, Inst Arctic & Alpine Res, Dept Geog, Campus Box 450 UCB, Boulder, CO 80309 USA.
EM leah.meromy@colorado.edu
RI Fassnacht, Steven/A-7742-2014; Molotch, Noah/C-8576-2009
OI Fassnacht, Steven/0000-0002-5270-8049;
FU NSF Hydrological Sciences [EAR1032295, EAR1032308]; NOAA Office of
Hydrologic Development [NA07NWS4620016]
FX This research was made possible by the NSF Hydrological Sciences (grant
nos. EAR1032295 and EAR1032308) and the NOAA Office of Hydrologic
Development (grant no. NA07NWS4620016). The authors thank their partners
at NOAA, including Tom Carroll, Don Cline, Carrie Olheiser, Andy Rost
and Pedro Restrepo. They also thank everyone who helped in the field.
NR 49
TC 30
Z9 30
U1 0
U2 27
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0885-6087
EI 1099-1085
J9 HYDROL PROCESS
JI Hydrol. Process.
PD AUG 15
PY 2013
VL 27
IS 17
BP 2383
EP 2400
DI 10.1002/hyp.9355
PG 18
WC Water Resources
SC Water Resources
GA 285ZA
UT WOS:000329432700001
ER
PT J
AU Jermwongratanachai, T
Jacobs, G
Ma, WP
Shafer, WD
Gnanamani, MK
Gao, P
Kitiyanan, B
Davis, BH
Klettlinger, JLS
Yen, CH
Cronauer, DC
Kropf, AJ
Marshall, CL
AF Jermwongratanachai, Thani
Jacobs, Gary
Ma, Wenping
Shafer, Wilson D.
Gnanamani, Muthu Kumaran
Gao, Pei
Kitiyanan, Boonyarach
Davis, Burtron H.
Klettlinger, Jennifer L. S.
Yen, Chia H.
Cronauer, Donald C.
Kropf, A. Jeremy
Marshall, Christopher L.
TI Fischer-Tropsch synthesis: Comparisons between Pt and Ag promoted
Co/Al2O3 catalysts for reducibility, local atomic structure, catalytic
activity, and oxidation-reduction (OR) cycles
SO APPLIED CATALYSIS A-GENERAL
LA English
DT Article
DE Fischer-Tropsch synthesis (FTS); Gas-to-liquids (GTL); Silver (Ag);
Platinum (Pt); Cobalt (Co); Co/Al2O3; XANES; EXAFS; Oxidation-reduction
(OR) cycles
ID WATER-GAS-SHIFT; IN-SITU EXAFS; COBALT ALUMINA CATALYSTS; SELECTIVE
HYDROGENATION; CARBON-MONOXIDE; RHENIUM; KINETICS; XPS; TPR;
SPECTROSCOPY
AB For economic reasons, Ag as a substitute for Pt promoter for FT Co/Al2O3 catalysts was advocated, due to its satisfactory ability to facilitate cobalt oxide reduction, its good catalytic performance in improving the CO conversion and selectivity and, especially, its much lower price compared to that of Pt (i.e., $23.31/Troy oz Ag. vs $1486.0/Troy oz Pt (May 10, 2013)). A comparative study between Pt and Ag promoters at several equivalent atomic loadings was performed in this work. While either Pt or Ag significantly facilitates cobalt oxide reduction supplying additional Co metal active sites compared to the unpromoted Co/Al2O3 catalysts, the total metal site density increased with increasing Pt loading, but become attenuated at high Ag loading. The EXAFS results indicate isolated Pt atoms interact with cobalt clusters to form Pt-Co bonds, without evidence of Pt-Pt bond formation, even at levels as high as 5 wt% Pt. In Ag promoted Co/Al2O3 catalyst, not only were Ag-Co bonds observed, but Ag-Ag bonds were present, even at levels as low as 0.276% Ag. The degree of Ag-Ag coordination increased as a function of Ag loading, while decreases in BET surface area and a shift to wider average pore size suggests some pore blocking by Ag at high loadings, which likely restricted access of reactants to internal cobalt sites. Therefore, although both promoters initially facilitate reduction of cobalt oxides, their local atomic structures are fundamentally different. Either Pt or Ag can significantly improve the CO conversion rate on a per gram catalyst basis of Co/Al2O3. Slightly adverse effects on selectivity (i.e., increased CH4 and CO2, at detriment to C-5+) were found with Pt, especially at higher loading, while Ag provides some benefits (i.e., slightly decreases CH4 and CO2, and increases C-5+) at all loadings tested in this work. Moreover, TPR and chemisorption/pulse reoxidation results show that Pt and Ag continue to be in proximity with Co following oxidation-reduction (OR) cycles to continue to facilitate reduction. Additional reaction tests are required to determine the impact of regeneration on performance. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Jermwongratanachai, Thani; Jacobs, Gary; Ma, Wenping; Shafer, Wilson D.; Gnanamani, Muthu Kumaran; Gao, Pei; Davis, Burtron H.] Univ Kentucky, Ctr Appl Energy Res, Lexington, KY 40511 USA.
[Jermwongratanachai, Thani; Kitiyanan, Boonyarach] Chulalongkorn Univ, Petr & Petrochem Coll, Bangkok 10330, Thailand.
[Gao, Pei] Eastern Kentucky Univ, Richmond, KY 40475 USA.
[Klettlinger, Jennifer L. S.; Yen, Chia H.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Cronauer, Donald C.; Kropf, A. Jeremy; Marshall, Christopher L.] Argonne Natl Lab, Argonne, IL 60439 USA.
RP Davis, BH (reprint author), Univ Kentucky, Ctr Appl Energy Res, 2540 Res Pk Dr, Lexington, KY 40511 USA.
EM burtron.davis@uky.edu
RI BM, MRCAT/G-7576-2011; Gnanamani, Muthu Kumaran/M-7736-2015; Marshall,
Christopher/D-1493-2015; Jacobs, Gary/M-5349-2015
OI Gnanamani, Muthu Kumaran/0000-0003-1274-2645; Marshall,
Christopher/0000-0002-1285-7648; Jacobs, Gary/0000-0003-0691-6717
FU NASA [NNX11AI75A]; Commonwealth of Kentucky; U.S. DOE, Office of Fossil
Energy, NETL; U.S. DOE, Office of Science, Office of Basic Energy
Sciences [DE-AC02-06CH11357]; DOE; MRCAT member institutions;
Fulbright-TRF scholarship program
FX CAER work was supported by a NASA grant (Relating FTS catalyst
properties to performance No. NNX11AI75A) and by the Commonwealth of
Kentucky. Argonne's research was supported in part by the U.S. DOE,
Office of Fossil Energy, NETL. The use of the APS was supported by the
U.S. DOE, Office of Science, Office of Basic Energy Sciences, under
Contract No. DE-AC02-06CH11357. MRCAT operations are supported by the
DOE and the MRCAT member institutions. We would like to thank Ms.
Shelley Hopps for her assistance with XRD experiments. We are also
grateful to the Fulbright-TRF scholarship program for financial support
for Mr. Thani Jermwongratanachai.
NR 37
TC 25
Z9 25
U1 10
U2 91
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0926-860X
EI 1873-3875
J9 APPL CATAL A-GEN
JI Appl. Catal. A-Gen.
PD AUG 15
PY 2013
VL 464
BP 165
EP 180
DI 10.1016/j.apcata.2013.05.040
PG 16
WC Chemistry, Physical; Environmental Sciences
SC Chemistry; Environmental Sciences & Ecology
GA 210BW
UT WOS:000323805300021
ER
PT J
AU Huang, XC
Fortenberry, RC
Wang, YM
Francisco, JS
Crawford, TD
Bowman, JM
Lee, TJ
AF Huang, Xinchuan
Fortenberry, Ryan C.
Wang, Yimin
Francisco, Joseph S.
Crawford, T. Daniel
Bowman, Joel M.
Lee, Timothy J.
TI Dipole Surface and Infrared Intensities for the cis- and trans-HOCO and
DOCO Radicals
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID SHELL HARTREE-FOCK; POTENTIAL-ENERGY SURFACE; VIBRATIONAL FREQUENCIES;
ROVIBRATIONAL ENERGIES; ELECTRON-AFFINITIES; INTERSTELLAR HOCO+;
GALACTIC-CENTER; WAVE-FUNCTIONS; BASIS-SETS; SPECTRUM
AB The vibrational spectra for the HOCO radical in both of its conformers and deuterated isotopologues are shown here for the first time. Building on previous work with coupled cluster quartic force fields (QFFs) in the computation of the fundamental vibrational frequencies for both cis- and trans-HOCO, coupled cluster dipole surfaces are now provided for both HOCO conformers and their corresponding deuterated isotopologues. These surfaces and subsequent vibrational configuration interaction (VCI) computations produce the intensities of transitions into vibrational states including the fundamentals, overtones, and first few combination bands of less than 4000 cm(-1), slightly beyond the O-H stretch. Simulated spectra with an artificial full width at half-maximum broadening of 10 cm(-1) are also provided in order to aid in the characterization of HOCO's vibrational frequencies and to assist detection in various laboratory or astronomical observations.
C1 [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
[Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wang, Yimin; Bowman, Joel M.] Emory Univ, Cherry L Emerson Ctr Sci Computat, Atlanta, GA 30322 USA.
[Wang, Yimin; Bowman, Joel M.] Emory Univ, Dept Chem, Atlanta, GA 30322 USA.
[Francisco, Joseph S.] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA.
[Fortenberry, Ryan C.; Crawford, T. Daniel] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA.
RP Huang, XC (reprint author), SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA.
EM Xinchuan.Huang-1@nasa.gov; Timothy.J.Lee@nasa.gov
RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013; Crawford,
Thomas/A-9271-2017
OI Crawford, Thomas/0000-0002-7961-7016
FU NASA [10-APRA10-0096, 10-APRA10-0167]; NASA/SETI Institute [NNX12AG96A];
U.S. National Science Foundation through a Multi-User Chemistry Research
Instrumentation and Facility (CRIF:MU) [CHE-0741927, CHE-1058420]; NASA;
Department of Energy [DE DFG02-97ER14782]
FX X.H. and T.J.L. are delighted to dedicate this work to Joel M. Bowman
Festschrift, on occasion of his 65th birthday, and gratefully
acknowledge the support, advice and collegiality that Professor Joel
Bowman has shown over the many years in which we have collaborated. The
work undertaken by X.H. and T.J.L. was made possible through NASA Grant
10-APRA10-0096 and 10-APRA10-0167. X.H. also acknowledges funding from
the NASA/SETI Institute Cooperative Agreement NNX12AG96A. The U.S.
National Science Foundation supported the work by R.C.F. and T.D.C.
through a Multi-User Chemistry Research Instrumentation and Facility
(CRIF:MU) Award CHE-0741927 and through Award CHE-1058420. R.C.F. was
also funded, in part, through the NASA Postdoctoral Program administered
by Oak Ridge Associated Universities. J.M.B. thanks the Department of
Energy (DE DFG02-97ER14782) for financial support. The artificial
broadening program used was provided by Dr. Micah Abrams of Abrams
Scientific Consulting.
NR 60
TC 16
Z9 16
U1 0
U2 23
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 AUG 15
PY 2013
VL 117
IS 32
BP 6932
EP 6939
DI 10.1021/jp3102546
PG 8
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 203NV
UT WOS:000323300800003
PM 23199284
ER
PT J
AU Lehnert, H
Stone, RP
AF Lehnert, Helmut
Stone, Robert P.
TI Four new species of Haplosclerida (Porifera, Demospongiae) from the
Aleutian Islands, Alaska
SO ZOOTAXA
LA English
DT Article
DE Callyspongiidae; Chalinidae; Callyspongia; Cladocroce; Aleutian Islands;
North Pacific; Alaska
AB Four new species of Haplosclerida are described from the Aleutian Islands, Alaska: Callyspongia mucosa n.sp., Cladocroce infundibulum n. sp., Cladocroce attu n. sp. and Cladocroce kiska n. sp. The new species are described and compared to congeners of the region. This is the northernmost record of the genus Callyspongia and the first record of the subgenus Callyspongia from the North Pacific Ocean. To accommodate Cladocroce kiska in its genus the definition has to be broadened to allow sigmas.
C1 [Stone, Robert P.] Natl Marine Fisheries Serv, Auke Bay Labs, Alaska Fisheries Sci Ctr, Juneau, AK 99801 USA.
RP Lehnert, H (reprint author), Eichenstr 14, D-86507 Oberottmarshausen, Germany.
EM Lehnert@spongetaxonomics.de; bob.stone@noaa.gov
FU Alaska Fisheries Science Center of NOAA/NMFS
FX We thank Jim Stark, Jay Orr and the crew of the FV Ocean Explorer for
collecting the specimens. Many thanks to the Zoologische Staatssammlung,
Munchen, for providing access to the SEM, especially thanks to Enrico
Schwabe for help operating the SEM. Light microscopical photos where
made at the Institute for Developmental Biology, University of Erlangen.
Thanks to Wolfgang Heimler for providing access. We thank David Drumm
(Alaska Fisheries Science Center, RACE) for providing Figure 1. Helmut
Lehnert was supported by a contract from the Alaska Fisheries Science
Center of NOAA/NMFS. We thank two anonymous reviewers for their helpful
comments. The findings and conclusions in this paper are those of the
authors and do not necessarily represent the views of the National
Marine Fisheries Service.
NR 20
TC 6
Z9 6
U1 1
U2 10
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 AUG 15
PY 2013
VL 3700
IS 4
BP 573
EP 582
PG 10
WC Zoology
SC Zoology
GA 200YD
UT WOS:000323106600005
PM 26106744
ER
PT J
AU Stecker, FW
AF Stecker, Floyd W.
TI PeV neutrinos observed by IceCube from cores of active galactic nuclei
SO PHYSICAL REVIEW D
LA English
DT Article
AB I show that the high energy neutrino flux predicted to arise from active galactic nuclei cores can explain the PeV neutrinos detected by IceCube without conflicting with the constraints from the observed extragalactic cosmic-ray and gamma-ray backgrounds.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Stecker, FW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Floyd.W.Stecker@nasa.gov
NR 10
TC 70
Z9 71
U1 0
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD AUG 15
PY 2013
VL 88
IS 4
AR 047301
DI 10.1103/PhysRevD.88.047301
PG 2
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 203UB
UT WOS:000323318000006
ER
PT J
AU Saleeb, AF
Kumar, A
Padula, SA
Dhakal, B
AF Saleeb, A. F.
Kumar, A.
Padula, S. A., II
Dhakal, B.
TI The cyclic and evolutionary response to approach the attraction loops
under stress controlled isothermal conditions for a multi-mechanism
based multi-axial SMA model
SO MECHANICS OF MATERIALS
LA English
DT Article
DE Shape memory alloy; Isothermal; Stress mean and amplitude; Cyclic
evolution; Attraction state; Multi-mechanism
ID SHAPE-MEMORY ALLOYS; MULTIVARIANT MICROMECHANICAL MODEL; INSPIRED
CONSTITUTIVE MODEL; HIGH STRAIN-RATE; POLYCRYSTALLINE SMAS; TI-NI;
PHASE-TRANSFORMATION; PART II; BEHAVIOR; DEFORMATION
AB The main focus in the present work has been on studying the evolutionary responses of Shape Memory Alloy (SMA) materials under isothermal, cyclic loading conditions. To this end, predictions of a recently-developed SMA material model by the authors is used here to carry out the qualitative comparisons to some of the available experimental results in the literature for SMA material responses under different uniaxial and multi-axial conditions of stress-control, both in the pseudoelastic and the pseudoplastic regimes. In the formulation of this model, the significant roles played by the internal state variables, underlying the inelastic mechanisms in the model to regulate the material's evolutionary response under extended cycles, are emphasized. The results presented have led to a number of important conclusions. First, the evolutionary character for pseudoelasticity is markedly different from that occurring in the pseudoplastic regime. Second, the virgin material response under minor loop cycles is dramatically different from its pre-cycled counterpart for which a prior major loop was established. Third, the careful selection of the loading-control variable such as magnitudes of the mean stress and stress amplitude plays a major role in dictating the amount of strain and detailed shapes of the saturated stress-strain loop achieved, as well as the number of cycles required to reach the saturation. Lastly, multi-axial load cycling under conditions of combined tension/compression/shear leads to a faster approach to the saturated states compared to the uniaxial load condition. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Saleeb, A. F.; Kumar, A.; Dhakal, B.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
[Padula, S. A., II] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Saleeb, AF (reprint author), Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
EM saleeb@uakron.edu
FU Fundamental Aeronautics Program, Subsonic, Fixed-Wing [NNH10ZEA001
N-SFW1, NNX11AI57A]
FX This work was supported by the Fundamental Aeronautics Program,
Subsonic, Fixed-Wing, Project No. NNH10ZEA001 N-SFW1, Grant No:
NNX11AI57A to the University of Akron. The authors would like to
acknowledge Drs. S.M. Arnold and Ronald Noebe for their technical
guidance and programmatic support during the different phases of the
project.
NR 63
TC 10
Z9 10
U1 1
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-6636
J9 MECH MATER
JI Mech. Mater.
PD AUG 15
PY 2013
VL 63
BP 21
EP 47
DI 10.1016/j.mechmat.2013.04.003
PG 27
WC Materials Science, Multidisciplinary; Mechanics
SC Materials Science; Mechanics
GA 174OU
UT WOS:000321166100003
ER
PT J
AU Burton, MG
Braiding, C
Glueck, C
Goldsmith, P
Hawkes, J
Hollenbach, DJ
Kulesa, C
Martin, CL
Pineda, JL
Rowell, G
Simon, R
Stark, AA
Stutzki, J
Tothill, NJH
Urquhart, JS
Walker, C
Walsh, AJ
Wolfire, M
AF Burton, Michael G.
Braiding, C.
Glueck, C.
Goldsmith, P.
Hawkes, J.
Hollenbach, D. J.
Kulesa, C.
Martin, C. L.
Pineda, J. L.
Rowell, G.
Simon, R.
Stark, A. A.
Stutzki, J.
Tothill, N. J. H.
Urquhart, J. S.
Walker, C.
Walsh, A. J.
Wolfire, M.
TI The Mopra Southern Galactic Plane CO Survey
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
LA English
DT Article
DE Galaxy: kinematics and dynamics; Galaxy: structure; ISM: clouds; ISM:
molecules; radio lines: ISM; surveys
ID GIANT MOLECULAR CLOUDS; GAMMA-RAY SIGNATURES; MILKY-WAY; STAR-FORMATION;
INTERSTELLAR CLOUDS; CARBON-MONOXIDE; OUTER GALAXY; RING SURVEY; DARK
GAS; EMISSION
AB We present the first results from a new carbon monoxide (CO) survey of the southern Galactic plane being conducted with the Mopra radio telescope in Australia. The (CO)-C-12, (CO)-C-13, and (CO)-O-18 J = 1-0 lines are being mapped over the l = 305 degrees-345 degrees, b= +/- 0.5 degrees portion of the fourth quadrant of the Galaxy, at 35 arcsec spatial and 0.1 km s(-1) spectral resolution. The survey is being undertaken with two principal science objectives: (i) to determine where and how molecular clouds are forming in the Galaxy and (ii) to probe the connection between molecular clouds and the 'missing' gas inferred from gamma-ray observations. We describe the motivation for the survey, the instrumentation and observing techniques being applied, and the data reduction and analysis methodology. In this paper, we present the data from the first degree surveyed, l = 323 degrees-324 degrees, b= +/- 0.5 degrees. We compare the data to the previous CO survey of this region and present metrics quantifying the performance being achieved; the rms sensitivity per 0.1 km s-1 velocity channel is similar to 1.5 K for (CO)-C-12 and similar to 0.7 K for the other lines. We also present some results from the region surveyed, including line fluxes, column densities, molecular masses, (CO)-C-12/(CO)-C-13 line ratios, and (CO)-C-12 optical depths. We also examine how these quantities vary as a function of distance from the Sun when averaged over the 1 square degree survey area. Approximately 2 x 10(6) M-circle dot of molecular gas is found along the G323 sightline, with an average H-2 number density of n(H2) similar to 1 cm(-3) within the Solar circle. The CO data cubes will be made publicly available as they are published.
C1 [Burton, Michael G.; Braiding, C.; Tothill, N. J. H.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Glueck, C.; Simon, R.; Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany.
[Goldsmith, P.; Pineda, J. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hawkes, J.; Rowell, G.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Hollenbach, D. J.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Kulesa, C.; Walker, C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Martin, C. L.] Oberlin Coll, Dept Phys & Astron, Oberlin, OH 44074 USA.
[Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Tothill, N. J. H.] Univ Western Sydney, Sch Comp Engn & Math, Penrith, NSW 2751, Australia.
[Urquhart, J. S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Walsh, A. J.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Wolfire, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Burton, MG (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
EM m.burton@unsw.edu.au
RI Walsh, Andrew/B-5627-2013;
OI Walsh, Andrew/0000-0001-9506-0855; Burton, Michael/0000-0001-7289-1998;
Rowell, Gavin/0000-0002-9516-1581; Stark, Antony/0000-0002-2718-9996
FU Commonwealth of Australia; Australian Research Council (ARC)
[DP120101585]
FX The Mopra radio telescope 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. Many staff of the ATNF have
contributed to the success of the remote operations at Mopra. We
particularly wish to acknowledge the contributions of David Brodrick,
Philip Edwards, Brett Hisock, Balt Indermuehle, and Peter Mirtschin. The
University of New South Wales Digital Filter Bank used for the
observations with the Mopra Telescope (the UNSW-MOPS) was provided with
support from the Australian Research Council (ARC). We also acknowledge
ARC support through Discovery Project DP120101585. This work was also
carried out, in part, at the Jet Propulsion Laboratory, California
Institute of Technology. Finally, we thank the anonymous referee whose
comments have helped improve this paper.
NR 65
TC 3
Z9 3
U1 0
U2 5
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1323-3580
EI 1448-6083
J9 PUBL ASTRON SOC AUST
JI Publ. Astron. Soc. Aust.
PD AUG 14
PY 2013
VL 30
AR e044
DI 10.1017/pasa.2013.22
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 201UU
UT WOS:000323169300001
ER
PT J
AU Li, LM
Achterberg, RK
Conrath, BJ
Gierasch, PJ
Smith, MA
Simon-Miller, AA
Nixon, CA
Orton, GS
Flasar, FM
Jiang, X
Baines, KH
Morales-Juberias, R
Ingersoll, AP
Vasavada, AR
Del Genio, AD
West, RA
Ewald, SP
AF Li, Liming
Achterberg, Richard K.
Conrath, Barney J.
Gierasch, Peter J.
Smith, Mark A.
Simon-Miller, Amy A.
Nixon, Conor A.
Orton, Glenn S.
Flasar, F. Michael
Jiang, Xun
Baines, Kevin H.
Morales-Juberias, Raul
Ingersoll, Andrew P.
Vasavada, Ashwin R.
Del Genio, Anthony D.
West, Robert A.
Ewald, Shawn P.
TI Strong Temporal Variation Over One Saturnian Year: From Voyager to
Cassini
SO SCIENTIFIC REPORTS
LA English
DT Article
ID CLOUD STRUCTURE; INFRARED SPECTROMETER; THERMAL STRUCTURE; EQUATORIAL
JET; RADIO SCIENCE; ATMOSPHERE; SYSTEM; WINDS; TEMPERATURES; OSCILLATION
AB Here we report the combined spacecraft observations of Saturn acquired over one Saturnian year (similar to 29.5 Earth years), from the Voyager encounters (1980-81) to the new Cassini reconnaissance (2009-10). The combined observations reveal a strong temporal increase of tropic temperature (similar to 10 Kelvins) around the tropopause of Saturn (i.e., 50 mbar), which is stronger than the seasonal variability (similar to a few Kelvins). We also provide the first estimate of the zonal winds at 750 mbar, which is close to the zonal winds at 2000 mbar. The quasi-consistency of zonal winds between these two levels provides observational support to a numerical suggestion inferring that the zonal winds at pressures greater than 500 mbar do not vary significantly with depth. Furthermore, the temporal variation of zonal winds decreases its magnitude with depth, implying that the relatively deep zonal winds are stable with time.
C1 [Li, Liming; Smith, Mark A.; Jiang, Xun] Univ Houston, Houston, TX 77204 USA.
[Achterberg, Richard K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Conrath, Barney J.; Gierasch, Peter J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Simon-Miller, Amy A.; Nixon, Conor A.; Flasar, F. Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Orton, Glenn S.; Baines, Kevin H.; Vasavada, Ashwin R.; West, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Morales-Juberias, Raul] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
[Ingersoll, Andrew P.; Ewald, Shawn P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Li, LM (reprint author), Univ Houston, Houston, TX 77204 USA.
EM lli7@central.uh.edu
RI Nixon, Conor/A-8531-2009; Flasar, F Michael/C-8509-2012; Simon,
Amy/C-8020-2012
OI Nixon, Conor/0000-0001-9540-9121; Simon, Amy/0000-0003-4641-6186
FU NASA Cassini Data Analysis and Outer Planets Research Programs
FX NASA Cassini Data Analysis and Outer Planets Research Programs funded
this work. We acknowledge the teams of Voyager (IRIS and ISS) and
Cassini (CIRS and ISS) for providing the data sets. We also thank the
anonymous reviewers for their constructive suggestions.
NR 36
TC 3
Z9 3
U1 0
U2 14
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 AUG 12
PY 2013
VL 3
AR 2410
DI 10.1038/srep02410
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 198XE
UT WOS:000322956000003
PM 23934437
ER
PT J
AU Acero, F
Ackermann, M
Ajello, M
Allafort, A
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Blandford, RD
Bloom, ED
Bonamente, E
Bottacini, E
Brandt, TJ
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Cecchi, C
Charles, E
Chaves, RCG
Chekhtman, A
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cutini, S
Dalton, M
D'Ammando, F
de Palma, F
Dermer, CD
Di Venere, L
Silva, EDE
Drell, PS
Drlica-Wagner, A
Falletti, L
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Franckowiak, A
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Gregoire, T
Grenier, IA
Grondin, MH
Grove, JE
Guiriec, S
Hadasch, D
Hanabata, Y
Harding, AK
Hayashida, M
Hayashi, K
Hays, E
Hewitt, J
Hill, AB
Horan, D
Hou, X
Hughes, RE
Inoue, Y
Jackson, MS
Jogler, T
Johannesson, G
Johnson, AS
Kamae, T
Kawano, T
Kerr, M
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Latronico, L
Lemoine-Goumard, M
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Marelli, M
Massaro, F
Mayer, M
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nakamori, T
Nemmen, R
Nuss, E
Ohsugi, T
Okumura, A
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Panetta, JH
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Reposeur, T
Ritz, S
Roth, M
Rousseau, R
Parkinson, PMS
Schulz, A
Sgro, C
Siskind, EJ
Smith, DA
Spandre, G
Spinelli, P
Suson, DJ
Takahashi, H
Takeuchi, Y
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Tibolla, O
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Uchiyama, Y
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Werner, M
Winer, BL
Wood, KS
Yang, Z
AF Acero, F.
Ackermann, M.
Ajello, M.
Allafort, A.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Bottacini, E.
Brandt, T. J.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Cecchi, C.
Charles, E.
Chaves, R. C. G.
Chekhtman, A.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cutini, S.
Dalton, M.
D'Ammando, F.
de Palma, F.
Dermer, C. D.
Di Venere, L.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Falletti, L.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Franckowiak, A.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Gregoire, T.
Grenier, I. A.
Grondin, M. -H.
Grove, J. E.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashida, M.
Hayashi, K.
Hays, E.
Hewitt, J.
Hill, A. B.
Horan, D.
Hou, X.
Hughes, R. E.
Inoue, Y.
Jackson, M. S.
Jogler, T.
Johannesson, G.
Johnson, A. S.
Kamae, T.
Kawano, T.
Kerr, M.
Knoedlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Latronico, L.
Lemoine-Goumard, M.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Marelli, M.
Massaro, F.
Mayer, M.
Mazziotta, M. N.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nakamori, T.
Nemmen, R.
Nuss, E.
Ohsugi, T.
Okumura, A.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Panetta, J. H.
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.
Ritz, S.
Roth, M.
Rousseau, R.
Parkinson, P. M. Saz
Schulz, A.
Sgro, C.
Siskind, E. J.
Smith, D. A.
Spandre, G.
Spinelli, P.
Suson, D. J.
Takahashi, H.
Takeuchi, Y.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Tibolla, O.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Uchiyama, Y.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Werner, M.
Winer, B. L.
Wood, K. S.
Yang, Z.
TI CONSTRAINTS ON THE GALACTIC POPULATION OF TeV PULSAR WIND NEBULAE USING
FERMI LARGE AREA TELESCOPE OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: general
ID GAMMA-RAY PULSARS; COMPOSITE SUPERNOVA REMNANT; YOUNG RADIO PULSAR;
ENERGETIC PSR J1357-6429; BLIND FREQUENCY SEARCHES; XMM-NEWTON
OBSERVATIONS; SOURCE HESS J1303-631; X-RAY; MAGNETIC-FIELD; CRAB-NEBULA
AB Pulsar wind nebulae (PWNe) have been established as the most populous class of TeV gamma-ray emitters. Since launch, the Fermi Large Area Telescope (LAT) has identified five high-energy (100 MeV < E < 100 GeV) gamma-ray sources as PWNe and detected a large number of PWN candidates, all powered by young and energetic pulsars. The wealth of multi-wavelength data available and the new results provided by Fermi-LAT give us an opportunity to find new PWNe and to explore the radiative processes taking place in known ones. The TeV gamma-ray unidentified (UNID) sources are the best candidates for finding new PWNe. Using 45 months of Fermi-LAT data for energies above 10 GeV, an analysis was performed near the position of 58 TeV PWNe and UNIDs within 5. of the Galactic plane to establish new constraints on PWN properties and find new clues on the nature of UNIDs. Of the 58 sources, 30 were detected, and this work provides their gamma-ray fluxes for energies above 10 GeV. The spectral energy distributions and upper limits, in the multi-wavelength context, also provide new information on the source nature and can help distinguish between emission scenarios, i.e., between classification as a pulsar candidate or as a PWN candidate. Six new GeV PWN candidates are described in detail and compared with existing models. A population study of GeV PWN candidates as a function of the pulsar/PWN system characteristics is presented.
C1 [Acero, F.; Brandt, T. J.; Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hays, E.; Hewitt, J.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ackermann, M.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Di Venere, L.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Massaro, F.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA.
[Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Di Venere, L.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Massaro, F.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, CNRS, Serv Astrophys, Lab AIM,CEA IRFU,CEA Saclay, 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.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain.
[Caraveo, P. A.; Marelli, M.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00044 Frascati, Italy.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Italy.
[Cohen-Tanugi, J.; Falletti, L.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier, France.
[Conrad, J.; Larsson, S.; Yang, Z.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.; Jackson, M. S.; Larsson, S.; Yang, Z.] Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden.
[Dalton, M.; Hou, X.; Lemoine-Goumard, M.; Mehault, J.; Reposeur, T.; Rousseau, R.; Smith, D. A.] Univ Bordeaux 1, CNRS, IN2p3, CEN Bordeaux Gradignan, F-33175 Gradignan, France.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Fukazawa, Y.; Hanabata, Y.; Hayashi, K.; Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Gregoire, T.; Grondin, M. -H.; Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Gregoire, T.; Grondin, M. -H.; Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, F-31028 Toulouse, France.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA.
[Jackson, M. S.] Royal Inst Technol KTH, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Nakamori, T.; Takeuchi, Y.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Okumura, A.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Razzano, M.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Razzano, M.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[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.
[Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Torres, D. F.] ICREA, E-08010 Barcelona, Spain.
[Vianello, G.] Consorzio Interuniv Fis Spaziale, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RP Acero, F (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM funk@slac.stanford.edu; joshualande@gmail.com; lemoine@cenbg.in2p3.fr;
rousseau@cenbg.in2p3.fr
RI Massaro, Francesco/L-9102-2016; Torres, Diego/O-9422-2016; Orlando,
E/R-5594-2016; Di Venere, Leonardo/C-7619-2017; Saz Parkinson, Pablo
Miguel/I-7980-2013; Moskalenko, Igor/A-1301-2007; Rando,
Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Sgro,
Carmelo/K-3395-2016; Reimer, Olaf/A-3117-2013; Morselli,
Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015;
Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015;
Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012
OI orienti, monica/0000-0003-4470-7094; Giroletti,
Marcello/0000-0002-8657-8852; Mazziotta, Mario
Nicola/0000-0001-9325-4672; Gasparrini, Dario/0000-0002-5064-9495;
Baldini, Luca/0000-0002-9785-7726; Marelli, Martino/0000-0002-8017-0338;
Massaro, Francesco/0000-0002-1704-9850; Torres,
Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X;
Inoue, Yoshiyuki/0000-0002-7272-1136; Caraveo,
Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214;
SPINELLI, Paolo/0000-0001-6688-8864; Rando,
Riccardo/0000-0001-6992-818X; Hill, Adam/0000-0003-3470-4834; Bastieri,
Denis/0000-0002-6954-8862; Pesce-Rollins, Melissa/0000-0003-1790-8018;
Moskalenko, Igor/0000-0001-6141-458X; Reimer, Olaf/0000-0001-6953-1385;
Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080;
Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco,
Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395;
giglietto, nicola/0000-0002-9021-2888
FU K. A. Wallenberg Foundation; European Community [ERC-StG-259391]; Marie
Curie IOF [275861]
FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant
from the K. A. Wallenberg Foundation.; Funded by contract ERC-StG-259391
from the European Community.; Funded by a Marie Curie IOF,
FP7/2007-2013, grant agreement No. 275861.
NR 159
TC 28
Z9 28
U1 0
U2 19
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2013
VL 773
IS 1
AR 77
DI 10.1088/0004-637X/773/1/77
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 193BN
UT WOS:000322531900077
ER
PT J
AU Bauer, JM
Grav, T
Blauvelt, E
Mainzer, AK
Masiero, JR
Stevenson, R
Kramer, E
Fernandez, YR
Lisse, CM
Cutri, RM
Weissman, PR
Dailey, JW
Masci, FJ
Walker, R
Waszczak, A
Nugent, CR
Meech, KJ
Lucas, A
Pearman, G
Wilkins, A
Watkins, J
Kulkarni, S
Wright, EL
AF Bauer, James M.
Grav, Tommy
Blauvelt, Erin
Mainzer, A. K.
Masiero, Joseph R.
Stevenson, Rachel
Kramer, Emily
Fernandez, Yan R.
Lisse, C. M.
Cutri, Roc M.
Weissman, Paul R.
Dailey, John W.
Masci, Frank J.
Walker, Russel
Waszczak, Adam
Nugent, Carrie R.
Meech, Karen J.
Lucas, Andrew
Pearman, George
Wilkins, Ashlee
Watkins, Jessica
Kulkarni, Shrinivas
Wright, Edward L.
CA WISE Team
PTF Team
TI CENTAURS AND SCATTERED DISK OBJECTS IN THE THERMAL INFRARED: ANALYSIS OF
WISE/NEOWISE OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; minor planets, asteroids: general
ID OUTER SOLAR-SYSTEM; JUPITER-FAMILY COMETS; KUIPER-BELT OBJECTS; MODEL
CALIBRATION; SURVEY-EXPLORER; DUST COMA; MAIN BELT; POPULATION;
ASTEROIDS; PLANETS
AB The Wide-field Infrared Survey Explorer (WISE) observed 52 Centaurs and scattered disk objects (SDOs) in the thermal infrared, including 15 new discoveries. We present analyses of these observations to estimate sizes and mean optical albedos. We find mean albedos of 0.08 +/- 0.04 for the entire data set. Thermal fits yield average beaming parameters of 0.9 +/- 0.2 that are similar for both SDO and Centaur sub-classes. Biased cumulative size distributions yield size-frequency distribution power law indices of similar to-1.7 +/- 0.3. The data also reveal a relation between albedo and color at the 3 sigma level. No significant relation between diameter and albedos is found.
C1 [Bauer, James M.; Blauvelt, Erin; Mainzer, A. K.; Masiero, Joseph R.; Stevenson, Rachel; Kramer, Emily; Weissman, Paul R.; Nugent, Carrie R.; Wilkins, Ashlee] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, James M.; Cutri, Roc M.; Dailey, John W.; Masci, Frank J.; Lucas, Andrew; Pearman, George] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Grav, Tommy] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Kramer, Emily; Fernandez, Yan R.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA.
[Lisse, C. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Walker, Russel] Monterey Inst Res Astron, Marina, CA 93933 USA.
[Waszczak, Adam] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Meech, Karen J.] Univ Hawaii, Inst Astron, Manoa, HI 96822 USA.
[Meech, Karen J.] Univ Hawaii, NASA Astrobiol Inst, Inst Astron, Manoa, HI 96822 USA.
[Pearman, George] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Wilkins, Ashlee] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Watkins, Jessica] Univ Calif Los Angeles, Inst Planets & Exoplanets, Los Angeles, CA 90095 USA.
[Kulkarni, Shrinivas] CALTECH, Div Math Phys & Astron, Pasadena, CA 91125 USA.
[Wright, Edward L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Bauer, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-401, Pasadena, CA 91109 USA.
EM bauer@scn.jpl.nasa.gov
RI Lisse, Carey/B-7772-2016;
OI Lisse, Carey/0000-0002-9548-1526; Blauvelt, Erin/0000-0002-2944-5818;
Fernandez, Yanga/0000-0003-1156-9721; Masiero,
Joseph/0000-0003-2638-720X
FU National Aeronautics and Space Administration; Planetary Science
Division of NASA; NASA through the NASA Astrobiology Institute through
the Office of Space Science [NNA09DA77A]; NASA Postdoctoral Program; JPL
graduate internship program
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. This publication also makes use of data products from
NEOWISE, which is a project of JPL/Caltech, funded by the Planetary
Science Division of NASA. This material is based in part upon work
supported by NASA through the NASA Astrobiology Institute under
Cooperative Agreement No. NNA09DA77A issued through the Office of Space
Science. R. Stevenson is supported by the NASA Postdoctoral Program, and
E. Kramer acknowledges her support through the JPL graduate internship
program. Data were based in part on observations obtained at the Hale
Telescope, Palomar Observatory, as part of a collaborative agreement
between the California Institute of Technology, its divisions Caltech
Optical Observatories, and the Jet Propulsion Laboratory (operated for
NASA). Also, this work is based in part on observations obtained at the
Southern Astrophysical Research (SOAR) telescope, which is a joint
project of the Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da
Republica Federativa do Brasil, the U. S. National Optical Astronomy
Observatory (NOAO), the University of North Carolina at Chapel Hill
(UNC), and Michigan State University (MSU), with time allocated through
NOAO. We thank the anonymous reviewer for the very helpful comments of
manuscript drafts.
NR 79
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U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2013
VL 773
IS 1
AR 22
DI 10.1088/0004-637X/773/1/22
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 193BN
UT WOS:000322531900022
ER
PT J
AU Chen, CTJ
Hickox, RC
Alberts, S
Brodwin, M
Jones, C
Murray, SS
Alexander, D
Assef, RJ
Brown, MJI
Dey, A
Forman, WR
Gorjian, V
Goulding, AD
Le Floc'h, E
Jannuzi, BT
Mullaney, JR
Pope, A
AF Chen, Chien-Ting J.
Hickox, Ryan C.
Alberts, Stacey
Brodwin, Mark
Jones, Christine
Murray, Stephen S.
Alexander, DavidM.
Assef, Roberto J.
Brown, Michael J. I.
Dey, Arjun
Forman, William R.
Gorjian, Varoujan
Goulding, Andrew D.
Le Floc'h, Emeric
Jannuzi, Buell T.
Mullaney, James R.
Pope, Alexandra
TI A CORRELATION BETWEEN STAR FORMATION RATE AND AVERAGE BLACK HOLE
ACCRETION IN STAR-FORMING GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: evolution; galaxies: starburst; infrared:
galaxies; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; FORMATION RATE
INDICATOR; QUASAR HOST GALAXIES; IRAC SHALLOW SURVEY; WIDE-FIELD SURVEY;
SIMILAR-TO 2.5; X-RAY SURVEY; FORMATION HISTORY; GOODS-HERSCHEL
AB We present a measurement of the average supermassive black hole accretion rate (BHAR) as a function of the star formation rate (SFR) for galaxies in the redshift range 0.25 < z < 0.8. We study a sample of 1767 far-IR-selected star-forming galaxies in the 9 deg(2) Bootes multi-wavelength survey field. The SFR is estimated using 250 mu m observations from the Herschel Space Observatory, for which the contribution from the active galactic nucleus (AGN) is minimal. In this sample, 121 AGNs are directly identified using X-ray or mid-IR selection criteria. We combined these detected AGNs and an X-ray stacking analysis for undetected sources to study the average BHAR for all of the star-forming galaxies in our sample. We find an almost linear relation between the average BHAR (in M-circle dot yr(-1)) and the SFR (in M-circle dot yr(-1)) for galaxies across a wide SFR range 0.85 < log SFR < 2.56 : logBHAR = (-3.72 +/- 0.52) + (1.05 +/- 0.33) log SFR. This global correlation between SFR and average BHAR is consistent with a simple picture in which SFR and AGN activity are tightly linked over galaxy evolution timescales.
C1 [Chen, Chien-Ting J.; Hickox, Ryan C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA.
[Alberts, Stacey; Pope, Alexandra] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Jones, Christine; Forman, William R.; Goulding, Andrew D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Alexander, DavidM.; Mullaney, James R.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Assef, Roberto J.; Gorjian, Varoujan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Dey, Arjun; Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Le Floc'h, Emeric; Mullaney, James R.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA, DSM,Irfu,CNRS,CE Saclay, F-91191 Gif Sur Yvette, France.
RP Chen, CTJ (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA.
EM ctchen@dartmouth.edu
RI Brown, Michael/B-1181-2015;
OI Brown, Michael/0000-0002-1207-9137; Chen,
Chien-Ting/0000-0002-4945-5079; Alexander, David/0000-0002-5896-6313;
Forman, William/0000-0002-9478-1682
FU Dartmouth Fellowship; Chandra grant [SP8-9001X, AR8-9017X]
FX We are grateful to the anonymous referee for the very careful reading of
the paper, and the suggestions that significantly improved this paper.
We thank our colleagues on the AGES, IRAC Shallow Survey, SDWFS, NDWFS,
and the XBootes teams, and the HerMES team for making the data publicly
available. The first Spitzer MIPS survey of the Bootes region was
obtained using GTO time provided by the Spitzer Infrared Spectrograph
Team (PI: James Houck) and by M. Rieke. We thank the collaborators in
that work for access to the 24 mu m catalog generated from those data by
Emeric Le Floc'h. We also thank Chris S. Kochanek for useful
discussions. C.-T.J.C was supported by a Dartmouth Fellowship. This work
was supported in part by Chandra grants SP8-9001X and AR8-9017X.
NR 92
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2013
VL 773
IS 1
AR 3
DI 10.1088/0004-637X/773/1/3
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 193BN
UT WOS:000322531900003
ER
PT J
AU Folatelli, G
Morrell, N
Phillips, MM
Hsiao, E
Campillay, A
Contreras, C
Castellon, S
Hamuy, M
Krzeminski, W
Roth, M
Stritzinger, M
Burns, CR
Freedman, WL
Madore, BF
Murphy, D
Persson, SE
Prieto, JL
Suntzeff, NB
Krisciunas, K
Anderson, JP
Forster, F
Maza, J
Pignata, G
Rojas, PA
Boldt, L
Salgado, F
Wyatt, P
Olivares, EF
Gal-Yam, A
Sako, M
AF Folatelli, Gaston
Morrell, Nidia
Phillips, Mark M.
Hsiao, Eric
Campillay, Abdo
Contreras, Carlos
Castellon, Sergio
Hamuy, Mario
Krzeminski, Wojtek
Roth, Miguel
Stritzinger, Maximilian
Burns, Christopher R.
Freedman, Wendy L.
Madore, Barry F.
Murphy, David
Persson, S. E.
Prieto, Jose L.
Suntzeff, Nicholas B.
Krisciunas, Kevin
Anderson, Joseph P.
Foerster, Francisco
Maza, Jose
Pignata, Giuliano
Rojas, P. Andrea
Boldt, Luis
Salgado, Francisco
Wyatt, Pamela
Olivares, Felipe E.
Gal-Yam, Avishay
Sako, Masao
TI SPECTROSCOPY OF TYPE Ia SUPERNOVAE BY THE CARNEGIE SUPERNOVA PROJECT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: distances and redshifts; supernovae: general; techniques:
spectroscopic
ID DELAYED-DETONATION MODELS; EARLY SPECTRAL EVOLUTION; DARK-ENERGY
CONSTRAINTS; PHOTOMETRY DATA RELEASE; LIGHT CURVES; ULTRAVIOLET
EXTINCTION; LUMINOSITY INDICATORS; MAXIMUM BRIGHTNESS; REDSHIFT;
DIVERSITY
AB This is the first release of optical spectroscopic data of low-redshift Type Ia supernovae (SNe Ia) by the Carnegie Supernova Project including 604 previously unpublished spectra of 93 SNe Ia. The observations cover a range of phases from 12 days before to over 150 days after the time of B-band maximum light. With the addition of 228 near-maximum spectra from the literature, we study the diversity among SNe Ia in a quantitative manner. For that purpose, spectroscopic parameters are employed such as expansion velocities from spectral line blueshifts and pseudo-equivalent widths (pW). The values of those parameters at maximum light are obtained for 78 objects, thus providing a characterization of SNe Ia that may help to improve our understanding of the properties of the exploding systems and the thermonuclear flame propagation. Two objects, namely, SNe 2005M and 2006is, stand out from the sample by showing peculiar Si Pi and S Pi velocities but otherwise standard velocities for the rest of the ions. We further study the correlations between spectroscopic and photometric parameters such as light-curve decline rate and color. In agreement with previous studies, we find that the pW of Si Pi absorption features are very good indicators of light-curve decline rate. Furthermore, we demonstrate that parameters such as pW2 (Si Pi 4130) and pW6 (Si Pi 5972) provide precise calibrations of the peak B-band luminosity with dispersions of approximate to 0.15 mag. In the search for a secondary parameter in the calibration of peak luminosity for SNe Ia, we find a approximate to 2 sigma-3 sigma correlation between B-band Hubble residuals and the velocity at maximum light of S Pi and Si Pi lines.
C1 [Folatelli, Gaston] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe Kavli IPMU, WPI, Kashiwa, Chiba 2778583, Japan.
[Morrell, Nidia; Phillips, Mark M.; Hsiao, Eric; Campillay, Abdo; Contreras, Carlos; Castellon, Sergio; Roth, Miguel] Carnegie Observ, Las Campanas Observ, La Serena, Chile.
[Hamuy, Mario; Anderson, Joseph P.; Foerster, Francisco; Maza, Jose] Univ Chile, Dept Astron, Santiago, Chile.
[Krzeminski, Wojtek] Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Stritzinger, Maximilian] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Burns, Christopher R.; Freedman, Wendy L.; Madore, Barry F.; Murphy, David; Persson, S. E.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Madore, Barry F.] CALTECH, Jet Prop Lab, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Prieto, Jose L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Suntzeff, Nicholas B.; Krisciunas, Kevin] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Pignata, Giuliano] Univ Andres Bello, Dept Ciencias Fis, Santiago, Santiago Rm, Chile.
[Rojas, P. Andrea] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile.
[Boldt, Luis] Univ Bonn, Argelander Inst Astron, D-53111 Bonn, Germany.
[Salgado, Francisco] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Wyatt, Pamela] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA.
[Olivares, Felipe E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Gal-Yam, Avishay] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Sako, Masao] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
RP Folatelli, G (reprint author), Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe Kavli IPMU, WPI, Kashiwa, Chiba 2778583, Japan.
EM gaston.folatelli@ipmu.jp
RI Hamuy, Mario/G-7541-2016; Maza, Jose/I-5722-2016;
OI Maza, Jose/0000-0003-2068-1328; stritzinger,
maximilian/0000-0002-5571-1833
FU World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan; NSF [AST-0306969, AST-0908886, AST-0607438, AST-1008343];
FONDECYT [3110042, 3110142, 11090421]; Millennium Center for Supernova
Science [P10-064-F]; Programa Bicentenario de Ciencia y Tecnologia de
CONICYT; Programa Iniciativa Cientifica Milenio de MIDEPLAN; Danish
Agency for Science and Technology and Innovation through a Sapere Aude
Level 2 grant; [23740175]
FX This research is supported by the World Premier International Research
Center Initiative (WPI Initiative), MEXT, Japan. G. F. acknowledges
financial support by Grant-in-Aid for Scientific Research for Young
Scientists (23740175). This material is based upon work supported by NSF
under grants AST-0306969, AST-0908886, AST-0607438, and AST-1008343. F.
F., J. A., and G. P. acknowledge support from FONDECYT through grants
3110042, 3110142, and 11090421. J.A., F. F, M. H., and G. P. acknowledge
support provided by the Millennium Center for Supernova Science through
grant P10-064-F (funded by "Programa Bicentenario de Ciencia y
Tecnologia de CONICYT" and "Programa Iniciativa Cientifica Milenio de
MIDEPLAN"). M. S. acknowledges the generous support provided by the
Danish Agency for Science and Technology and Innovation through a Sapere
Aude Level 2 grant.
NR 97
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2013
VL 773
IS 1
AR 53
DI 10.1088/0004-637X/773/1/53
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 193BN
UT WOS:000322531900053
ER
PT J
AU Gandhi, P
Terashima, Y
Yamada, S
Mushotzky, RF
Ueda, Y
Baumgartner, WH
Alexander, DM
Malzac, J
Vaghmare, K
Takahashi, T
Done, C
AF Gandhi, P.
Terashima, Y.
Yamada, S.
Mushotzky, R. F.
Ueda, Y.
Baumgartner, W. H.
Alexander, D. M.
Malzac, J.
Vaghmare, K.
Takahashi, T.
Done, C.
TI REFLECTION-DOMINATED NUCLEAR X-RAY EMISSION IN THE EARLY-TYPE GALAXY ESO
565-G019
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; X-rays: galaxies; X-rays: individual (ESO 565-G019,
ESO 565-G018)
ID ACTIVE GALACTIC NUCLEI; SEYFERT 2 GALAXIES; ALL-SKY SURVEY; XMM-NEWTON;
BLACK-HOLES; HOST GALAXY; OPTICAL CLASSIFICATION; OBSCURED ACCRETION;
INFRARED GALAXIES; REDSHIFT SURVEY
AB We present the discovery of a reflection-dominated active galactic nucleus (AGN) in the early-type radio-quiet galaxy ESO 565-G019 with Suzaku and Swift/Burst Alert Telescope. The source X-ray spectrum below 10 keV is characteristic of other Compton-thick (CT) AGNs, clearly showing an inverted continuum and prodigious fluorescence iron emission above similar to 3 keV. A Compton shoulder to the neutral Fe K alpha line also appears to be present. There is evidence for long-term hard X-ray flux variability that we associate with changes in the intrinsic AGN power law. More of such reflection-dominated AGNs should be uncovered in the near future with the increased sensitivity of ongoing and new hard X-ray surveys. ESO 565-G019 is hosted in an early-type galaxy whose morphology has been variously classified as either type E or type S0. Only about 20 bona fide CT-AGNs have been identified in the local universe so far, and all exist in host galaxies with late Hubble types (S0 or later). CT columns of nuclear obscuring gas are uncommon in early-type galaxies in the local universe, so confirmation of the exact morphological class of ESO 565-G019 is important. Infrared photometry also shows the presence of large quantities of cool dust in the host, indicative of significant ongoing star formation. ESO 565-G019 may be the first identified local example of minor-merger-driven CT-AGN growth in an early-type host, or may be the result of interaction with its neighboring galaxy ESO 565-G018 in a wide pair.
C1 [Gandhi, P.; Takahashi, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Gandhi, P.; Alexander, D. M.; Done, C.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Terashima, Y.] Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan.
[Yamada, S.] RIKEN, Cosm Radiat Lab, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan.
[Mushotzky, R. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Ueda, Y.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Baumgartner, W. H.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Malzac, J.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France.
[Malzac, J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Vaghmare, K.] IUCAA, Pune 411007, Maharashtra, India.
[Takahashi, T.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
RP Gandhi, P (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
RI XRAY, SUZAKU/A-1808-2009; done, chris/D-4605-2016;
OI done, chris/0000-0002-1065-7239; Alexander, David/0000-0002-5896-6313
FU JAXA; STFC [ST/J00369711]; NASA; National Science Foundation
FX P.G. acknowledges support from JAXA and STFC (grant reference
ST/J00369711). The authors thank Suzaku team members. K. V. thanks Y.
Wadadekar and S. Barway for enlightening discussions. P. G. thanks S. F.
Honig for comments. Swift/BAT transient monitor data are used herein.
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. WISE is a project of University of California,
Los Angeles, and Jet Propulsion Laboratory (JPL)/California Institute of
Technology (Caltech), funded by the NASA. 2MASS is a project of the
University of Massachusetts and the Infrared Processing and Analysis
Center/Caltech funded by NASA and the National Science Foundation. Akari
is a project of the Japan Aerospace Exploration Agency with the
participation of the European Space Agency. The NASA/IPAC Infrared
Science Archive (IRSA) operated by JPL under contract with NASA was used
for querying the infrared databases. The HyperLEDA database was also
useful in this work. The reviewer provided constructive criticisms that
improved the paper. The Suzaku data used herein are available from the
publicly open data archive at JAXA.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2013
VL 773
IS 1
AR UNSP 51
DI 10.1088/0004-637X/773/1/51
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 193BN
UT WOS:000322531900051
ER
PT J
AU Janson, M
Brandt, TD
Moro-Martin, A
Usuda, T
Thalmann, C
Carson, JC
Goto, M
Currie, T
McElwain, MW
Itoh, Y
Fukagawa, M
Crepp, J
Kuzuhara, M
Hashimoto, J
Kudo, T
Kusakabe, N
Abe, L
Brandner, W
Egner, S
Feldt, M
Grady, CA
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Kandori, R
Knapp, GR
Kwon, J
Matsuo, T
Miyama, S
Morino, JI
Nishimura, T
Pyo, TS
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, Y
Takami, M
Takato, N
Terada, H
Tomono, D
Turner, EL
Watanabe, M
Wisniewski, J
Yamada, T
Takami, H
Tamura, M
AF Janson, Markus
Brandt, Timothy D.
Moro-Martin, Amaya
Usuda, Tomonori
Thalmann, Christian
Carson, Joseph C.
Goto, Miwa
Currie, Thayne
McElwain, M. W.
Itoh, Yoichi
Fukagawa, Misato
Crepp, Justin
Kuzuhara, Masayuki
Hashimoto, Jun
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Abe, Lyu
Brandner, Wolfgang
Egner, Sebastian
Feldt, Markus
Grady, Carol A.
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiro
Hayashi, Saeko
Henning, Thomas
Hodapp, Klaus W.
Ishii, Miki
Iye, Masanori
Kandori, Ryo
Knapp, Gillian R.
Kwon, Jungmi
Matsuo, Taro
Miyama, Shoken
Morino, Jun-Ichi
Nishimura, Tetsuro
Pyo, Tae-Soo
Serabyn, Eugene
Suenaga, Takuya
Suto, Hiroshi
Suzuki, Ryuji
Takahashi, Yasuhiro
Takami, Michihiro
Takato, Naruhisa
Terada, Hiroshi
Tomono, Daego
Turner, Edwin L.
Watanabe, Makoto
Wisniewski, John
Yamada, Toru
Takami, Hideki
Tamura, Motohide
TI THE SEEDS DIRECT IMAGING SURVEY FOR PLANETS AND SCATTERED DUST EMISSION
IN DEBRIS DISK SYSTEMS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems; stars: early-type
ID SUN-LIKE STARS; SPITZER-SPACE-TELESCOPE; LOW-MASS STARS; CIRCUMSTELLAR
DISK; BETA-PICTORIS; EPSILON-ERIDANI; GIANT PLANETS; SCORPIUS-CENTAURUS;
BROWN DWARFS; EVOLUTIONARY MODELS
AB Debris disks around young main-sequence stars often have gaps and cavities which for a long time have been interpreted as possibly being caused by planets. In recent years, several giant planet discoveries have been made in systems hosting disks of precisely this nature, further implying that interactions with planets could be a common cause of such disk structures. As part of the SEEDS high-contrast imaging survey, we are surveying a population of debris-disk-hosting stars with gaps and cavities implied by their spectral energy distributions, in order to attempt to spatially resolve the disk as well as to detect any planets that may be responsible for the disk structure. Here, we report on intermediate results from this survey. Five debris disks have been spatially resolved, and a number of faint point sources have been discovered, most of which have been tested for common proper motion, which in each case has excluded physical companionship with the target stars. From the detection limits of the 50 targets that have been observed, we find that beta Pic b-like planets (similar to 10 M-jup planets around G-A-type stars) near the gap edges are less frequent than 15%-30%, implying that if giant planets are the dominant cause of these wide (27 AU on average) gaps, they are generally less massive than beta Pic b.
C1 [Janson, Markus; Brandt, Timothy D.; Knapp, Gillian R.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Moro-Martin, Amaya] CAB INTA CSIC, Dept Astrophys, E-28850 Madrid, Spain.
[Usuda, Tomonori; Kudo, Tomoyuki; Egner, Sebastian; Guyon, Olivier; Hayano, Yutaka; Hayashi, Masahiro; Hayashi, Saeko; Ishii, Miki; Nishimura, Tetsuro; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daego; Takami, Hideki] Subaru Telescope, Hilo, HI 96720 USA.
[Thalmann, Christian] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Carson, Joseph C.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Carson, Joseph C.; Brandner, Wolfgang; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Goto, Miwa] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Currie, Thayne] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[McElwain, M. W.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 2071 USA.
[Itoh, Yoichi] Univ Hyogo, Ctr Astron, Nishi Harima Astron Observ, Sayo, Hyogo 6795313, Japan.
[Fukagawa, Misato] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Crepp, Justin] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Kuzuhara, Masayuki; Hashimoto, Jun; Kusakabe, Nobuhiko; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Suto, Hiroshi; Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7239, F-06300 Nice, France.
[Grady, Carol A.] Eureka Sci, Oakland, CA 96002 USA.
[Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Kwon, Jungmi; Suenaga, Takuya] Grad Univ Adv Studies Sokendai, Dept Astron Sci, Tokyo 1818588, Japan.
[Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Miyama, Shoken] Hiroshima Univ, Off President, Hagashi Hiroshima 7398511, Japan.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Suzuki, Ryuji] TMT Observ Corp, Pasadena, CA 91105 USA.
[Takahashi, Yasuhiro] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan.
[Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Yamada, Toru] Tohoku Univ, Astron Inst, Sendai, Miyagi 9808578, Japan.
RP Janson, M (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
EM janson@astro.princeton.edu
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
FU NASA through Hubble Fellowship [HF-51290.01]; Space Telescope Science
Institute; NSF [1009203]; NASA [NAS 5-26555]
FX Support for this work was provided by NASA through Hubble Fellowship
grant HF-51290.01 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. J.C. was
supported by NSF award 1009203. Archival data from the Subaru, Gemini,
Keck and Hubble telescopes have been used as part of this study. We
acknowledge the cultural significance of Mauna Kea to the indigenous
population of Hawaii. This study made use of the CDS services SIMBAD and
VizieR, as well as the SAO/NASA ADS service.
NR 116
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2013
VL 773
IS 1
AR 73
DI 10.1088/0004-637X/773/1/73
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 193BN
UT WOS:000322531900073
ER
PT J
AU Loewenstein, M
AF Loewenstein, Michael
TI PERSPECTIVES ON INTRACLUSTER ENRICHMENT AND THE STELLAR INITIAL MASS
FUNCTION IN ELLIPTICAL GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: intracluster medium;
galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies:
formation; galaxies: star formation; galaxies: stellar content
ID STAR-FORMATION RATE; DELAY-TIME DISTRIBUTION; CORE-COLLAPSE SUPERNOVAE;
INTRA-CLUSTER MEDIUM; X-RAY OBSERVATIONS; GALACTIC CHEMICAL EVOLUTION;
TO-LIGHT RATIOS; IA SUPERNOVAE; ELEMENTAL ABUNDANCES; METAL ENRICHMENT
AB Stars formed in galaxy cluster potential wells must be responsible for the high level of enrichment measured in the intracluster medium (ICM); however, there is increasing tension between this truism and the parsimonious assumption that the stars in the generally old population studied optically in cluster galaxies emerged from the same formation sites at the same epochs. We construct a phenomenological cluster enrichment model to demonstrate that ICM elemental abundances are underestimated by a factor >2 for standard assumptions about the stellar population-a discrepancy we call the "cluster elemental abundance paradox." Recent evidence of an elliptical galaxy initial mass function (IMF) skewed to low masses deepens the paradox. We quantify the adjustments to the star formation efficiency and IMF, and Type Ia supernovae (SNIa) production efficiency, required to resolve this while being consistent with the observed ICM abundance pattern. The necessary enhancement in metal enrichment may, in principle, originate in the observed stellar population if a larger fraction of stars in the supernova-progenitor mass range form from an IMF that is either bottom-light or top-heavy, with the latter in some conflict with observed ICM abundance ratios. Other alternatives that imply more modest revisions to the IMF, mass return and remnant fractions, and primordial fraction, posit an increase in the fraction of 3-8 M-circle dot stars that explode as SNIa or assume that there are more stars than conventionally thought-although the latter implies a high star formation efficiency. We discuss the feasibility of these various solutions and the implications for the diversity of star formation in the universe, the process of elliptical galaxy formation, and the origin of this "hidden" source of ICM metal enrichment.
C1 [Loewenstein, Michael] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Loewenstein, Michael] NASA, GSFC, CRESST, Greenbelt, MD USA.
[Loewenstein, Michael] NASA, GSFC, Xray Astrophys Lab, Greenbelt, MD USA.
RP Loewenstein, M (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM Michael.Loewenstein.1@nasa.gov
NR 136
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U1 1
U2 12
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 AUG 10
PY 2013
VL 773
IS 1
AR 52
DI 10.1088/0004-637X/773/1/52
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 193BN
UT WOS:000322531900052
ER
PT J
AU Martin, RG
Armitage, PJ
Alexander, RD
AF Martin, Rebecca G.
Armitage, Philip J.
Alexander, Richard D.
TI FORMATION OF CIRCUMBINARY PLANETS IN A DEAD ZONE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; binaries: close; planets and satellites:
formation; protoplanetary disks; stars: pre-main sequence
ID T TAURI DISKS; PROTOPLANETARY DISCS; ACCRETION DISKS; PLANETESIMAL
ACCRETION; CIRCUMSTELLAR DISKS; LAYERED ACCRETION; MILLIMETER EMISSION;
TURBULENT DISKS; BINARY-SYSTEMS; STAR SYSTEMS
AB Circumbinary planets have been observed at orbital radii where binary perturbations may have significant effects on the gas disk structure, on planetesimal velocity dispersion, and on the coupling between turbulence and planetesimals. Here, we note that the impact of all of these effects on planet formation is qualitatively altered if the circumbinary disk structure is layered, with a non-turbulent midplane layer (dead zone) and strongly turbulent surface layers. For close binaries, we find that the dead zone typically extends from a radius close to the inner disk edge up to a radius of around 10-20AU from the center of mass of the binary. The peak in the surface density occurs within the dead zone, far from the inner disk edge, close to the snow line, and may act as a trap for aerodynamically coupled solids. We suggest that circumbinary planet formation may be easier near this preferential location than for disks around single stars. However, dead zones around wide binaries are less likely, and hence planet formation may be more difficult there.
C1 [Martin, Rebecca G.; Armitage, Philip J.] Univ Colorado, JILA, Boulder, CO 80309 USA.
[Martin, Rebecca G.; Armitage, Philip J.] NIST, Boulder, CO 80309 USA.
[Armitage, Philip J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Alexander, Richard D.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
RP Martin, RG (reprint author), NASA, Washington, DC 20546 USA.
FU California Institute of Technology (Caltech); NASA through the Sagan
Fellowship Program; NASA [HST-AR-12814, NAS 5-26555]; Space Telescope
Science Institute; NASA's Origins of Solar Systems program [NNX13AI58G];
Science and Technology Facilities Council (STFC) through an Advanced
Fellowship [ST/G00711X/1, ST/K001000/1]
FX We thank an anonymous referee for useful comments. R.G.M.'s support was
provided in part under contract with the California Institute of
Technology (Caltech) funded by NASA through the Sagan Fellowship
Program. P.J.A. acknowledges support from NASA under grant HST-AR-12814
awarded by the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., for
NASA, under contact NAS 5-26555, and from NASA's Origins of Solar
Systems program under grant NNX13AI58G. R.D.A. acknowledges support from
the Science and Technology Facilities Council (STFC) through an Advanced
Fellowship (ST/G00711X/1) and Consolidated grant ST/K001000/1.
NR 79
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2013
VL 773
IS 1
AR 74
DI 10.1088/0004-637X/773/1/74
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 193BN
UT WOS:000322531900074
ER
PT J
AU Rhoads, JE
Malhotra, S
Stern, D
Dickinson, M
Pirzkal, N
Spinrad, H
Reddy, N
Hathi, N
Grogin, N
Koekemoer, A
Peth, MA
Cohen, S
Zheng, ZY
Budavari, T
Ferreras, I
Gardner, JP
Gronwall, C
Haiman, Z
Kummel, M
Meurer, G
Moustakas, L
Panagia, N
Pasquali, A
Sahu, K
Alighieri, SD
Somerville, R
Straughn, A
Walsh, J
Windhorst, R
Xu, C
Yan, HJ
AF Rhoads, James E.
Malhotra, Sangeeta
Stern, Daniel
Dickinson, Mark
Pirzkal, Norbert
Spinrad, Hyron
Reddy, Naveen
Hathi, Nimish
Grogin, Norman
Koekemoer, Anton
Peth, Michael A.
Cohen, Seth
Zheng, Zhenya
Budavari, Tamas
Ferreras, Ignacio
Gardner, Jonathan P.
Gronwall, Caryl
Haiman, Zoltan
Kuemmel, Martin
Meurer, Gerhardt
Moustakas, Leonidas
Panagia, Nino
Pasquali, Anna
Sahu, Kailash
Alighieri, Sperello di Serego
Somerville, Rachel
Straughn, Amber
Walsh, Jeremy
Windhorst, Rogier
Xu, Chun
Yan, Haojing
TI A LYMAN BREAK GALAXY IN THE EPOCH OF REIONIZATION FROM HUBBLE SPACE
TELESCOPE GRISM SPECTROSCOPY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift
ID LY-ALPHA EMITTERS; ULTRA DEEP FIELD; SIMILAR-TO 7; EXTRAGALACTIC LEGACY
SURVEY; LUMINOSITY FUNCTION; EMITTING GALAXIES; KECK SPECTROSCOPY;
SLITLESS SPECTROSCOPY; WFC3/IR OBSERVATIONS; CANDIDATE GALAXIES
AB We present observations of a luminous galaxy at z = 6.573-the end of the reionization epoch-which has been spectroscopically confirmed twice. The first spectroscopic confirmation comes from slitless Hubble Space Telescope Advanced Camera for Surveys grism spectra from the PEARS survey (Probing Evolution And Reionization Spectroscopically), which show a dramatic continuum break in the spectrum at rest frame 1216 angstrom. The second confirmation is done with Keck + DEIMOS. The continuum is not clearly detected with ground-based spectra, but high wavelength resolution enables the Ly alpha emission line profile to be determined. We compare the line profile to composite line profiles at z = 4.5. The Ly alpha line profile shows no signature of a damping wing attenuation, confirming that the intergalactic gas is ionized at z = 6.57. Spectra of Lyman breaks at yet higher redshifts will be possible using comparably deep observations with IR-sensitive grisms, even at redshifts where Ly alpha is too attenuated by the neutral intergalactic medium to be detectable using traditional spectroscopy from the ground.
C1 [Rhoads, James E.; Malhotra, Sangeeta; Cohen, Seth; Zheng, Zhenya; Windhorst, Rogier] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Stern, Daniel; Moustakas, Leonidas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dickinson, Mark] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Pirzkal, Norbert; Grogin, Norman; Koekemoer, Anton; Peth, Michael A.; Panagia, Nino; Sahu, Kailash] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Spinrad, Hyron] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Reddy, Naveen] Univ Calif Riverside, Riverside, CA 92521 USA.
[Hathi, Nimish] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Peth, Michael A.; Budavari, Tamas] Johns Hopkins Univ, Baltimore, MD USA.
[Ferreras, Ignacio] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Gardner, Jonathan P.; Straughn, Amber] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Gronwall, Caryl] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Gronwall, Caryl] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Haiman, Zoltan] Columbia Univ, New York, NY USA.
[Kuemmel, Martin] Univ Sternwarte, D-81679 Munich, Germany.
[Meurer, Gerhardt] Univ Western Australia, Int Ctr Radio Astron Res, Nedlands, WA 6009, Australia.
[Panagia, Nino; Alighieri, Sperello di Serego] INAF Osservatorio Astrofis Catania, Catania, Italy.
[Pasquali, Anna] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Somerville, Rachel] Rutgers State Univ, Piscataway, NJ USA.
[Walsh, Jeremy] European So Observ, Garching, Germany.
[Xu, Chun] Acad Sinica, Shanghai Inst Tech Phys, Shanghai 200083, Peoples R China.
[Yan, Haojing] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
RP Rhoads, JE (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM James.Rhoads@asu.edu
RI Hathi, Nimish/J-7092-2014
OI Ferreras, Ignacio/0000-0003-4584-3127; Koekemoer,
Anton/0000-0002-6610-2048; Moustakas, Leonidas/0000-0003-3030-2360; di
Serego Alighieri, Sperello/0000-0001-8769-2692; Hathi,
Nimish/0000-0001-6145-5090
FU STScI [HST-GO-10530]; NASA [NAS 5-26555]; Eberly College of Science;
Office of the Senior Vice President for Research at the Pennsylvania
State University; W. M. Keck Foundation
FX J.E.R. and S.M. thank the DARK Cosmology Centre and Nordea-fonden in
Copenhagen, Denmark, and Anri's Place in Betalbatim, India, for
hospitality during the completion of this work. We thank Mauro
Giavalisco and the GOODS team for providing early access to GOODS v1.9
and v2.0 images to help with spectroscopic extractions. We thank
Emanuele Daddi for his contributions to the PEARS project. This work has
been supported by grant HST-GO-10530 from STScI, which is operated by
AURA for NASA under contract NAS 5-26555. The work of D. S. was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. The Institute for Gravitation
and the Cosmos is supported by the Eberly College of Science and the
Office of the Senior Vice President for Research at the Pennsylvania
State University. Some data presented herein were obtained at the W. M.
Keck Observatory. The Observatory was made possible by the generous
financial support of the W. M. Keck Foundation. The authors 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.
NR 57
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2013
VL 773
IS 1
AR 32
DI 10.1088/0004-637X/773/1/32
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 193BN
UT WOS:000322531900032
ER
PT J
AU Wilkes, BJ
Kuraszkiewicz, J
Haas, M
Barthel, P
Leipski, C
Willner, SP
Worrall, DM
Birkinshaw, M
Antonucci, R
Ashby, MLN
Chini, R
Fazio, GG
Lawrence, C
Ogle, P
Schulz, B
AF Wilkes, Belinda J.
Kuraszkiewicz, Joanna
Haas, Martin
Barthel, Peter
Leipski, Christian
Willner, S. P.
Worrall, D. M.
Birkinshaw, Mark
Antonucci, Robert
Ashby, M. L. N.
Chini, Rolf
Fazio, G. G.
Lawrence, Charles
Ogle, Patrick
Schulz, Bernhard
TI REVEALING THE HEAVILY OBSCURED ACTIVE GALACTIC NUCLEUS POPULATION OF
HIGH-REDSHIFT 3CRR SOURCES WITH CHANDRA X-RAY OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE quasars: general; X-rays: galaxies
ID COMPACT STEEP-SPECTRUM; XMM-NEWTON OBSERVATIONS; POWERFUL RADIO
GALAXIES; DIGITAL SKY SURVEY; EXTRAGALACTIC LEGACY SURVEY;
DUAL-FREQUENCY OBSERVATIONS; SUPERMASSIVE BLACK-HOLES; EXTENDED GROTH
STRIP; SEYFERT 2 GALAXIES; DEEP FIELD SOUTH
AB Chandra observations of a complete, flux-limited sample of 38 high-redshift (1 < z < 2), low-frequency-selected (and so unbiased in orientation) 3CRR radio sources are reported. The sample includes 21 quasars (=broad-line radio galaxies) and 17 narrow-line radio galaxies (NLRGs) with matched 178 MHz radio luminosity (log L-R(5 GHz) similar to 44-45). The quasars have high radio core fraction, high X-ray luminosities (log L-X similar to 45-46), and soft X-ray hardness ratios (HR similar to -0.5) indicating low obscuration. The NLRGs have lower core fraction, lower apparent X-ray luminosities (log L-X similar to 43-45), and mostly hard X-ray hardness ratios (HR > 0) indicating obscuration (N-H similar to 10(22)-10(24) cm(-2)). These properties and the correlation between obscuration and radio core fraction are consistent with orientation-dependent obscuration as in unification models. About half the NLRGs have soft X-ray hardness ratios and/or a high [O III] emission line to X-ray luminosity ratio suggesting obscuration by Compton thick (CT) material so that scattered nuclear or extended X-ray emission dominates (as in NGC 1068). The ratios of unobscured to Compton-thin (10(22) cm(-2) < N-H(int) < 1.5 x 10(24) cm(-2)) to CT (N-H(int) > 1.5 x 10(24) cm(-2)) is 2.5:1.4:1 in this high-luminosity, radio-selected sample. The obscured fraction is 0.5, higher than is typically reported for active galactic nuclei at comparable luminosities from multi-wavelength surveys (0.1-0.3). Assuming random nuclear orientation, the unobscured half-opening angle of the disk/wind/torus structure is similar to 60 degrees and the obscuring material covers 30 degrees, similar to 12 degrees of which is CT. The multi-wavelength properties reveal that many NLRGs have intrinsic absorption 10-1000x higher than indicated by their X-ray hardness ratios, and their true L-X values are similar to 10-100x larger than the hardness-ratio absorption corrections would indicate.
C1 [Wilkes, Belinda J.; Kuraszkiewicz, Joanna; Willner, S. P.; Ashby, M. L. N.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Haas, Martin; Chini, Rolf] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany.
[Barthel, Peter] Univ Groningen, Kapteyn Inst, NL-9747 AD Groningen, Netherlands.
[Leipski, Christian] MPIA, D-69117 Heidelberg, Germany.
[Worrall, D. M.; Birkinshaw, Mark] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Antonucci, Robert] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Chini, Rolf] Univ Catolica Norte, Inst Astron, Antofagasta, Chile.
[Lawrence, Charles] JPL, Pasadena, CA 91109 USA.
[Ogle, Patrick] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Schulz, Bernhard] CALTECH, IPAC, Pasadena, CA 91125 USA.
RP Wilkes, BJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Wilkes, Belinda/0000-0003-1809-2364
FU National Aeronautics and Space Administration [G08-9106X, NAS8-03060];
Chandra X-Ray Center; Smithsonian Institution Endowment, Scholarly
Studies Program [40488100HH0017]
FX Support for this work was provided by the National Aeronautics and Space
Administration through Chandra Award Number G08-9106X, by the Chandra
X-Ray Center, which is operated by the Smithsonian Astrophysical
Observatory for and on behalf of the National Aeronautics Space
Administration under contract NAS8-03060 (Chandra X-Ray Center) and by
the Smithsonian Institution Endowment, Scholarly Studies Program, fund
40488100HH0017. The scientific results in this article are based to a
significant degree on observations made by the Chandra X-Ray Observatory
(CXO). We thank Mark Avara and Margaret Yellen for their early work on
this project.
NR 161
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2013
VL 773
IS 1
AR 15
DI 10.1088/0004-637X/773/1/15
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 193BN
UT WOS:000322531900015
ER
PT J
AU Zeng, LZ
Bennett, CL
Chapman, NL
Chuss, DT
Jimenez-Serra, I
Novak, G
Vaillancourt, JE
AF Zeng, Lingzhen
Bennett, Charles L.
Chapman, Nicholas L.
Chuss, David T.
Jimenez-Serra, Izaskun
Novak, Giles
Vaillancourt, John E.
TI THE SUBMILLIMETER POLARIZATION SPECTRUM OF M17
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: individual objects (M17, NGC 6618); ISM: magnetic
fields; polarization; submillimeter: ISM
ID MAGNETIC-FIELDS; GRAIN ALIGNMENT; MOLECULAR CLOUDS; INFRARED
POLARIZATION; INTERSTELLAR GRAINS; RADIATIVE TORQUES; GALACTIC CLOUDS;
SHARC-II; EMISSION; ORION
AB We present 450 mu m polarimetric observations of the M17 molecular cloud obtained with the SHARP polarimeter at the Caltech Submillimeter Observatory. Across the observed region, the magnetic field orientation is consistent with previous submillimeter and far-infrared polarization measurements. Our observations are centered on a region of the molecular cloud that has been compressed by stellar winds from a cluster of OB stars. We have compared these new data with previous 350 mu m polarimetry and find an anti-correlation between the 450 and 350 mu m polarization magnitude ratio and the ratio of 21 cm to 450 mu m intensity. The polarization ratio is lower near the east end of the studied region where the cloud is exposed to stellar winds and radiation. At the west end of the region, the polarization ratio is higher. We interpret the varying polarization spectrum as evidence supporting the radiative alignment torque model for grain alignment, implying higher alignment efficiency in the region that is exposed to a higher anisotropic radiation field.
C1 [Zeng, Lingzhen; Jimenez-Serra, Izaskun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zeng, Lingzhen; Bennett, Charles L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Chapman, Nicholas L.; Novak, Giles] Northwestern Univ, CIERA, Evanston, IL 60208 USA.
[Chapman, Nicholas L.; Novak, Giles] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Chuss, David T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Vaillancourt, John E.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Univ Space Res Assoc, Moffett Field, CA 94035 USA.
RP Zeng, LZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM lingzhen@cfa.harvard.edu
OI Vaillancourt, John/0000-0001-8916-1828; Zeng,
Lingzhen/0000-0001-6924-9072
FU National Science Foundation [AST-0838261, AST-0909030]
FX We thank C. Brogan for providing the 21 cm intensity data. We are
grateful to A. Chepurnov, R. Hildebrand, and A. Lazarian for
illuminating discussions. This material is based upon work at the
Caltech Submillimeter Observatory, which is operated by the California
Institute of Technology under cooperative agreement with the National
Science Foundation (AST-0838261). We thank the National Science
Foundation for supporting SHARP, via grant AST-0909030 to Northwestern
University.
NR 36
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2013
VL 773
IS 1
AR 29
DI 10.1088/0004-637X/773/1/29
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 193BN
UT WOS:000322531900029
ER
PT J
AU Axelsson, M
Fantaye, Y
Hansen, FK
Banday, AJ
Eriksen, HK
Gorski, KM
AF Axelsson, M.
Fantaye, Y.
Hansen, F. K.
Banday, A. J.
Eriksen, H. K.
Gorski, K. M.
TI DIRECTIONAL DEPENDENCE OF Lambda CDM COSMOLOGICAL PARAMETERS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmic background radiation; cosmology: observations; methods:
statistical
ID MICROWAVE-ANISOTROPY-PROBE; WMAP DATA; POWER-SPECTRUM
AB We study hemispherical power asymmetry in the Wilkinson Microwave Anisotropy Probe 9 yr data. We analyze the combined V- and W-band sky maps, after application of the KQ85 mask, and find that the asymmetry is statistically significant at the 3.4 sigma confidence level for l = 2-600, where the data are signal-dominated, with a preferred asymmetry direction (l, b) = (227,-27). Individual asymmetry axes estimated from six independent multipole ranges are all consistent with this direction. Subsequently, we estimate cosmological parameters on different parts of the sky and show that the parameters A(s), n(s), and Omega(b) are the most sensitive to this power asymmetry. In particular, for the two opposite hemispheres aligned with the preferred asymmetry axis, we find n(s) = 0.959 +/- 0.022 and n(s) = 0.989 +/- 0.024, respectively.
C1 [Axelsson, M.; Fantaye, Y.; Hansen, F. K.; Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Banday, A. J.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Gorski, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Gorski, K. M.] CALTECH, Pasadena, CA 91125 USA.
RP Axelsson, M (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, N-0315 Oslo, Norway.
EM magnus.axelsson@astro.uio.no; y.t.fantaye@astro.uio.no
FU Norwegian research council; ERC [StG2010-257080]; NASA office for Space
Science
FX F.K.H. acknowledges OYI grant from the Norwegian research council. H. K.
E. acknowledges support through the ERC Starting Grant StG2010-257080.
We acknowledge the use of resources from the Norwegian national super
computing facilities NOTUR. Maps and results have been derived using the
HEALpix (http://healpix.jpl.nasa.gov) software package developed by
Gorski et al. (2005). Results have been derived using the CosmoMC code
from Lewis & Bridle (2002). We acknowledge the use of the LAMBDA archive
(Legacy Archive for Microwave Background Data Analysis). Support for
LAMBDA is provided by the NASA office for Space Science.
NR 13
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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 AUG 10
PY 2013
VL 773
IS 1
AR L3
DI 10.1088/2041-8205/773/1/L3
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 192AF
UT WOS:000322455600003
ER
PT J
AU Bhattacharyya, B
Roy, J
Ray, PS
Gupta, Y
Bhattacharya, D
Romani, RW
Ransom, SM
Ferrara, EC
Wolff, MT
Camilo, F
Cognard, I
Harding, AK
den Hartog, PR
Johnston, S
Keith, M
Kerr, M
Michelson, PF
Parkinson, PMS
Wood, DL
Wood, KS
AF Bhattacharyya, B.
Roy, J.
Ray, P. S.
Gupta, Y.
Bhattacharya, D.
Romani, R. W.
Ransom, S. M.
Ferrara, E. C.
Wolff, M. T.
Camilo, F.
Cognard, I.
Harding, A. K.
den Hartog, P. R.
Johnston, S.
Keith, M.
Kerr, M.
Michelson, P. F.
Parkinson, P. M. Saz
Wood, D. L.
Wood, K. S.
TI GMRT DISCOVERY OF PSR J1544+4937: AN ECLIPSING BLACK-WIDOW PULSAR
IDENTIFIED WITH A FERMI-LAT SOURCE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: eclipsing; pulsars: general; pulsars: individual (PSR
J1544+4937)
ID LARGE-AREA TELESCOPE; MILLISECOND PULSAR; BINARY; CATALOG
AB Using the Giant Metrewave Radio Telescope, we performed deep observations to search for radio pulsations in the directions of unidentified Fermi-Large Area Telescope gamma-ray sources. We report the discovery of an eclipsing black-widow millisecond pulsar, PSR J1544+4937, identified with the uncataloged gamma-ray source Fermi J1544.2+4941. This 2.16 ms pulsar is in a 2.9 hr compact circular orbit with a very low mass companion (M-c > 0.017 M-circle dot). At 322 MHz this pulsar is found to be eclipsing for 13% of its orbit, whereas at 607 MHz the pulsar is detected throughout the low-frequency eclipse phase. Variations in the eclipse ingress phase are observed, indicating a clumpy and variable eclipsing medium. Moreover, additional short-duration absorption events are observed around the eclipse boundaries. Using the radio timing ephemeris we were able to detect gamma-ray pulsations from this pulsar, confirming it as the source powering the gamma-ray emission.
C1 [Bhattacharyya, B.; Roy, J.; Gupta, Y.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
[Ray, P. S.; Wolff, M. T.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Bhattacharya, D.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Romani, R. W.; den Hartog, P. R.; Kerr, M.; Michelson, P. F.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Romani, R. W.; den Hartog, P. R.; Kerr, M.; Michelson, P. F.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Ransom, S. M.] NRAO, Charlottesville, VA 22903 USA.
[Ferrara, E. C.; Harding, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Camilo, F.] Arecibo Observ, Arecibo, PR 00612 USA.
[Cognard, I.] CNRS, LPCE, UMR 6115, F-45071 Orleans 02, France.
[Cognard, I.] CNRS, INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France.
[Johnston, S.; Keith, M.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA.
[Wood, D. L.] Naval Res Lab, Washington, DC 20375 USA.
RP Bhattacharyya, B (reprint author), Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
RI Saz Parkinson, Pablo Miguel/I-7980-2013; Bhattacharya,
Dipankar/J-6927-2015;
OI Bhattacharya, Dipankar/0000-0003-3352-3142; Ransom,
Scott/0000-0001-5799-9714; Ray, Paul/0000-0002-5297-5278
FU NASA; DOE in the United States; CEA/Irfu; IN2P3/CNRS in France; ASI;
INFN in Italy; MEXT; KEK; JAXA in Japan; K. A. Wallenberg Foundation;
Swedish Research Council; National Space Board in Sweden; INAF in Italy;
CNES in France
FX The Fermi-LAT Collaboration acknowledges support from a number of
agencies and institutes for both development and the operation of the
LAT as well as scientific data analysis. These include NASA and DOE in
the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in
Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg
Foundation, the Swedish Research Council, and the National Space Board
in Sweden. Additional support from INAF in Italy and CNES in France for
science analysis during the operations phase is also gratefully
acknowledged. We acknowledge the support of the telescope operators of
the GMRT, which is run by the National Centre for Radio Astrophysics of
the Tata Institute of Fundamental Research. We thank the Swift team at
the Pennsylvania State University, especially Abe Falcone. We
acknowledge help of C. Cheung in interpreting the XRT data. We thank D.
Thompson and T. Johnson for their comments and R. Breton for a
discussion of heating fluxes.
NR 22
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 10
PY 2013
VL 773
IS 1
AR L12
DI 10.1088/2041-8205/773/1/L12
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 192AF
UT WOS:000322455600012
ER
PT J
AU Phifer, K
Do, T
Meyer, L
Ghez, AM
Witzel, G
Yelda, S
Boehle, A
Lu, JR
Morris, MR
Becklin, EE
Matthews, K
AF Phifer, K.
Do, T.
Meyer, L.
Ghez, A. M.
Witzel, G.
Yelda, S.
Boehle, A.
Lu, J. R.
Morris, M. R.
Becklin, E. E.
Matthews, K.
TI KECK OBSERVATIONS OF THE GALACTIC CENTER SOURCE G2: GAS CLOUD OR STAR?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; black hole physics; Galaxy: center; Galaxy:
kinematics and dynamics; infrared: general
ID SGR-A-ASTERISK; ADAPTIVE OPTICS SYSTEM; BLACK-HOLE; PROPER MOTIONS;
STELLAR ORBITS; CENTRAL PARSEC; YOUNG STARS; GALAXY; ACCRETION; DYNAMICS
AB We present new observations and analysis of G2-the intriguing red emission-line object which is quickly approaching the Galaxy's central black hole. The observations were obtained with the laser guide star adaptive optics systems on the W. M. Keck I and II telescopes (2006-2012) and include spectroscopy (R similar to 3600) centered on the hydrogen Br gamma line as well as K' (2.1 mu m) and L' (3.8 mu m) imaging. Analysis of these observations shows the Br gamma line emission has a positional offset from the L' continuum. This offset is likely due to background source confusion at L'. We therefore present the first orbital solution derived from Br gamma line astrometry, which, when coupled with radial velocity measurements, results in a later time of closest approach (2014.21 +/- 0.14), closer periastron (130 AU, 1600 R-s), and higher eccentricity (0.9814 +/- 0.0060) compared to a solution using L' astrometry. It is shown that G2 has no K' counterpart down to K' similar to 20 mag. G2's L' continuum and the Br gamma line emission appears unresolved in almost all epochs, which implies that the bulk of the emission resides in a compact region. The observations altogether suggest that while G2 has a gaseous component that is tidally interacting with the central black hole, there is likely a central star providing the self-gravity necessary to sustain the compact nature of this object.
C1 [Phifer, K.; Meyer, L.; Ghez, A. M.; Witzel, G.; Yelda, S.; Boehle, A.; Morris, M. R.; Becklin, E. E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Do, T.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Lu, J. R.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Becklin, E. E.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Matthews, K.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
EM ghez@astro.ucla.edu
OI Lu, Jessica/0000-0001-9611-0009; Do, Tuan/0000-0001-9554-6062
FU NSF [AST-0909218]; Keck Foundation
FX The authors acknowledge the invaluable feedback from the referee and
conference attendees at workshops where this work has been presented
(AAS 221st Meeting, Keck 20th Anniversary Celebration, Galactic Nuclei
Ringberg Workshop). Support for this work was provided by NSF grant
AST-0909218. Data presented herein were taken at the Keck Observatory,
which is operated as a scientific partnership among Caltech, UC, and
NASA; the Observatory was made possible by the generous financial
support of the Keck Foundation.
NR 38
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 10
PY 2013
VL 773
IS 1
AR L13
DI 10.1088/2041-8205/773/1/L13
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 192AF
UT WOS:000322455600013
ER
PT J
AU Teodoro, M
Madura, TI
Gull, TR
Corcoran, MF
Hamaguchi, K
AF Teodoro, M.
Madura, T. I.
Gull, T. R.
Corcoran, M. F.
Hamaguchi, K.
TI DETECTION OF THE COMPRESSED PRIMARY STELLAR WIND IN eta CARINAE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: general; stars: individual (eta Carinae); stars: massive
ID COLLIDING WINDS; ATOMIC DATABASE; EMISSION; HOMUNCULUS; CHIANTI
AB A series of three Hubble Space Telescope/Space Telescope Imaging Spectrograph spectroscopic mappings, spaced approximately one year apart, reveal three partial arcs in [Fe II] and [Ni II] emissions moving outward from eta Carinae. We identify these arcs with the shell-like structures, seen in the three-dimensional hydrodynamical simulations, formed by compression of the primary wind by the secondary wind during periastron passages.
C1 [Teodoro, M.; Madura, T. I.; Gull, T. R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Corcoran, M. F.; Hamaguchi, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Corcoran, M. F.; Hamaguchi, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Hamaguchi, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
EM mairan.teodoro@nasa.gov
FU CNPq/MCT-Brazil [201978/2012-1]; NASA
FX We are grateful to an anonymous referee for comments and suggestions
that helped to improve the quality and presentation of this work. M. T.
is supported by CNPq/MCT-Brazil through grant 201978/2012-1. T. I. M.
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. We thank Don Lindler for his
consistent help with the IDL procedures necessary for production of the
data cubes. M. T. would like to thank David Fanning for making his IDL
Coyote library (http://www.idlcoyote.com/index.html) publicly available.
CHIANTI is a collaborative project involving George Mason University,
the University of Michigan (USA) and the University of Cambridge (UK).
This research has made extensive use of NASA's Astrophysics Data System
and IDL Astronomy User's Library (http://idlastro.gsfc.nasa.gov/).
NR 17
TC 8
Z9 8
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 10
PY 2013
VL 773
IS 1
AR L16
DI 10.1088/2041-8205/773/1/L16
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 192AF
UT WOS:000322455600016
ER
PT J
AU Netzer, NL
Tanaka, Z
Chen, B
Jiang, CY
AF Netzer, Nathan L.
Tanaka, Zuki
Chen, Bin
Jiang, Chaoyang
TI Tailoring the SERS Enhancement Mechanisms of Silver Nanowire
Langmuir-Blodgett Films via Galvanic Replacement Reaction
SO JOURNAL OF PHYSICAL CHEMISTRY C
LA English
DT Article
ID RAMAN-SCATTERING; SINGLE-MOLECULE; P-AMINOTHIOPHENOL; SURFACE;
SPECTROSCOPY; NANOSTRUCTURES; AU; IDENTIFICATION; NANOPARTICLES;
MONOLAYERS
AB We report a new facile route for preparing surface-enhanced Raman scattering (SEAS) substrates with tailored enhancement mechanisms. Silver nanowires were assembled using the Langmuir-Blodgett (LB) technique and further processed via galvanic replacement reactions (GRRs). The GRRs provided an efficient method to decrease the spectral noise caused by the capping agent polyvinylpyrrolidone. A decrease in noise along with the addition of gold nanostructures to the system revealed Raman signals from nonfluorescent molecules associated with a charge-transfer mechanism. The GRR LB substrates exhibited ultrasensitive SERS ability with a detection limit as low as 8 nM using 4-aminothiophenol, partially due to the strong chemical binding between the SERS substrates and probe molecules. Furthermore, the GRRs provide a facile route in tailoring SERS substrates to target molecules in a controlled manner.
C1 [Netzer, Nathan L.; Jiang, Chaoyang] Univ S Dakota, Dept Chem, Vermillion, SD 57069 USA.
[Tanaka, Zuki; Chen, Bin] NASA, Adv Studies Labs, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Jiang, CY (reprint author), Univ S Dakota, Dept Chem, 414 East Clark St, Vermillion, SD 57069 USA.
EM chaoyang.jiang@usd.edu
FU NSF [EPS-0903804, DGE-0903685]; NASA [NNX10AN34A]; State of South
Dakota; US Department of Energy [DE-EE0000270]
FX This research was supported by the NSF (EPS-0903804 and DGE-0903685),
NASA (Cooperative Agreement Number: NNX10AN34A), and by the State of
South Dakota. Purchase of the LB trough was made possible through the US
Department of Energy, contract number DE-EE0000270. We thank Ms. Tam Ho
for sample preparation and valuable discussions. We also appreciate the
anonymous referees for their valuable comments and suggestions.
NR 41
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U1 5
U2 59
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 AUG 8
PY 2013
VL 117
IS 31
BP 16187
EP 16194
DI 10.1021/jp405796b
PG 8
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA 200PV
UT WOS:000323082300039
ER
PT J
AU Hedman, MM
Gosmeyer, CM
Nicholson, PD
Sotin, C
Brown, RH
Clark, RN
Baines, KH
Buratti, BJ
Showalter, MR
AF Hedman, M. M.
Gosmeyer, C. M.
Nicholson, P. D.
Sotin, C.
Brown, R. H.
Clark, R. N.
Baines, K. H.
Buratti, B. J.
Showalter, M. R.
TI An observed correlation between plume activity and tidal stresses on
Enceladus
SO NATURE
LA English
DT Article
ID WATER RESERVOIR; CASSINI ISS; SOUTH-POLE; E-RING; SPECTROMETER;
ERUPTIONS; ORIGIN; VIMS; MASS
AB Saturn's moon Enceladus emits a plume of water vapour and micrometre-sized ice particles from a series of warm fissures located near its south pole(1-10). This geological activity could be powered or controlled by variations in the tidal stresses experienced by Enceladus as it moves around its slightly eccentric orbit. The specific mechanisms by which these varying stresses are converted into heat, however, are still being debated(11-16). Furthermore, it has proved difficult to find a clear correlation between the predicted tidal forces and measured temporal variations in the plume's gas content(17-19) or the particle flux from individual sources(20,21). Here we report that the plume's horizontally integrated brightness is several times greater when Enceladus is near the point in its eccentric orbit where it is furthest from Saturn (apocentre) than it is when near the point of closest approach to the planet (pericentre). More material therefore seems to be escaping from beneath Enceladus' surface at times when geophysical models predict its fissures should be under tension(12,15,16) and therefore may be wider open.
C1 [Hedman, M. M.; Nicholson, P. D.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Gosmeyer, C. M.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA.
[Sotin, C.; Baines, K. H.; Buratti, B. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brown, R. H.] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Clark, R. N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA.
[Showalter, M. R.] SETI Inst, Mountain View, CA 94043 USA.
RP Hedman, MM (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
EM mmhedman@astro.cornell.edu
FU VIMS team; Cassini project; NASA [NNX12AC29G]; Cornell University
FX We acknowledge the support of the VIMS team, the Cassini project and
NASA. This work was supported in part by NASA grant NNX12AC29G. The work
of C.M.G. on this project was made possible by the Research Experience
for Undergraduates programme at Cornell University.
NR 23
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U1 4
U2 33
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD AUG 8
PY 2013
VL 500
IS 7461
BP 182
EP 184
DI 10.1038/nature12371
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 197CH
UT WOS:000322825500029
PM 23903658
ER
PT J
AU Essick, R
Blackburn, L
Katsavounidis, E
AF Essick, R.
Blackburn, L.
Katsavounidis, E.
TI Optimizing vetoes for gravitational-wave transient searches
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
ID INSPIRAL TRIGGERS; LIGO DATA; BURSTS
AB Interferometric gravitational-wave detectors like LIGO, GEO600 and Virgo record a surplus of information above and beyond possible gravitational-wave events. These auxiliary channels capture information about the state of the detector and its surroundings which can be used to infer potential terrestrial noise sources of some gravitational-wave-like events. We present an algorithm addressing the ordering (or equivalently optimizing) of such information from auxiliary systems in gravitational-wave detectors to establish veto conditions in searches for gravitational-wave transients. The procedure was used to identify vetoes for searches for unmodeled transients by the LIGO and Virgo collaborations during their science runs from 2005 through 2007. In this work we present the details of the algorithm; we also use a limited amount of data from LIGO's past runs in order to examine the method, compare it with other methods, and identify its potential to characterize the instruments themselves. We examine the dependence of receiver operating characteristic curves on the various parameters of the veto method and the implementation on real data. We find that themethod robustly determines important auxiliary channels, ordering them by the apparent strength of their correlations to the gravitational-wave channel. This list can substantially reduce the background of noise events in the gravitational-wave data. In this way it can identify the source of glitches in the detector as well as assist in establishing confidence in the detection of gravitational-wave transients.
C1 [Essick, R.; Katsavounidis, E.] MIT, LIGO Lab, Cambridge, MA 02139 USA.
[Blackburn, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Essick, R (reprint author), MIT, LIGO Lab, NW22-295,185 Albany Str, Cambridge, MA 02139 USA.
EM ressick@mit.edu; lindy.l.blackburn@nasa.gov; kats@mit.edu
FU National Science Foundation; LIGO Laboratory; National Science
Foundation [PHY-0757058]; NASA Postdoctoral Program at Goddard Space
Flight Center
FX RE and EK gratefully acknowledge the support of the National Science
Foundation and the LIGO Laboratory. LIGO was constructed by the
California Institute of Technology and Massachusetts Institute of
Technology with funding from the National Science Foundation and
operates under cooperative agreement PHY-0757058. LB is supported by an
appointment to the NASA Postdoctoral Program at Goddard Space Flight
Center, administered by Oak Ridge Associated Universities through a
contract with NASA. The authors would also like to acknowledge comments
and feedback received by members of the Bursts, Compact Binary
Coalescences and Detector Characterization working groups of the LIGO
Scientific Collaboration and the Virgo Collaboration, as well as the
entire LIGO Scientific Collaboration and Virgo Collaboration for access
to this data. This paper has been assigned LIGO document number
LIGO-P1300038.
NR 21
TC 6
Z9 6
U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD AUG 7
PY 2013
VL 30
IS 15
AR 155010
DI 10.1088/0264-9381/30/15/155010
PG 18
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 181TY
UT WOS:000321692600011
ER
PT J
AU Wang, WL
Ciais, P
Nemani, RR
Canadell, JG
Piao, SL
Sitch, S
White, MA
Hashimoto, H
Milesi, C
Myneni, RB
AF Wang, Weile
Ciais, Philippe
Nemani, Ramakrishna R.
Canadell, Josep G.
Piao, Shilong
Sitch, Stephen
White, Michael A.
Hashimoto, Hirofumi
Milesi, Cristina
Myneni, Ranga B.
TI Variations in atmospheric CO2 growth rates coupled with tropical
temperature
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE climate-carbon cycle coupling; tropical land surface temperature; global
dynamic vegetation model
ID NET PRIMARY PRODUCTION; CARBON-DIOXIDE; INTERANNUAL VARIABILITY;
SOUTHERN-OSCILLATION; EQUATORIAL PACIFIC; CLIMATE-CHANGE; RAIN-FOREST;
EL-NINO; DROUGHT; LAND
AB Previous studies have highlighted the occurrence and intensity of El Nino-Southern Oscillation as important drivers of the interannual variability of the atmospheric CO2 growth rate, but the underlying biogeophysical mechanisms governing such connections remain unclear. Here we show a strong and persistent coupling (r(2) approximate to 0.50) between interannual variations of the CO2 growth rate and tropical land-surface air temperature during 1959 to 2011, with a 1 degrees C tropical temperature anomaly leading to a 3.5 +/- 0.6 Petagrams of carbon per year (PgC/y) CO2 growth-rate anomaly on average. Analysis of simulation results from Dynamic Global Vegetation Models suggests that this temperature-CO2 coupling is contributed mainly by the additive responses of heterotrophic respiration (Rh) and net primary production (NPP) to temperature variations in tropical ecosystems. However, we find a weaker and less consistent (r(2) approximate to 0.25) interannual coupling between CO2 growth rate and tropical land precipitation than diagnosed from the Dynamic Global Vegetation Models, likely resulting from the subtractive responses of tropical Rh and NPP to precipitation anomalies that partly offset each other in the net ecosystem exchange (i.e., net ecosystem exchange approximate to Rh - NPP). Variations in other climate variables (e.g., large-scale cloudiness) and natural disturbances (e.g., volcanic eruptions) may induce transient reductions in the temperature-CO2 coupling, but the relationship is robust during the past 50 y and shows full recovery within a few years after any such major variability event. Therefore, it provides an important diagnostic tool for improved understanding of the contemporary and future global carbon cycle.
C1 [Wang, Weile; Hashimoto, Hirofumi; Milesi, Cristina] Calif State Univ Monterey Bay, Div Sci & Environm Policy, Seaside, CA 93955 USA.
[Wang, Weile; Hashimoto, Hirofumi; Milesi, Cristina] NASA, Biospher Sci Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ciais, Philippe] Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France.
[Nemani, Ramakrishna R.] NASA, Adv Supercomp Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Canadell, Josep G.] Commonwealth Sci & Ind Res Org Marine & Atmospher, Global Carbon Project, Canberra, ACT 2601, Australia.
[Piao, Shilong] Peking Univ, Dept Ecol, Beijing 100871, Peoples R China.
[Sitch, Stephen] Univ Exeter, Dept Geog, Exeter EX4 4RJ, Devon, England.
[Piao, Shilong] Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing 100085, Peoples R China.
[White, Michael A.] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA.
[Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
RP Wang, WL (reprint author), Calif State Univ Monterey Bay, Div Sci & Environm Policy, Seaside, CA 93955 USA.
EM weile.wang@nasa.gov
RI Myneni, Ranga/F-5129-2012; Sitch, Stephen/F-8034-2015; Canadell,
Josep/E-9419-2010;
OI Sitch, Stephen/0000-0003-1821-8561; Canadell, Josep/0000-0002-8788-3218;
White, Michael/0000-0002-0238-8913
NR 59
TC 33
Z9 34
U1 7
U2 99
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 AUG 6
PY 2013
VL 110
IS 32
BP 13061
EP 13066
DI 10.1073/pnas.1219683110
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 196JQ
UT WOS:000322771100055
PM 23884654
ER
PT J
AU Wu, XF
Rahman, A
Zhou, ZP
Pelot, DD
Sinha-Ray, S
Chen, B
Payne, S
Yarin, AL
AF Wu, Xiang-Fa
Rahman, Arifur
Zhou, Zhengping
Pelot, David D.
Sinha-Ray, Suman
Chen, Bin
Payne, Scott
Yarin, Alexander L.
TI Electrospinning core-shell nanofibers for interfacial toughening and
self-healing of carbon-fiber/epoxy composites
SO JOURNAL OF APPLIED POLYMER SCIENCE
LA English
DT Article
DE electrospinning; fibers; mechanical properties; nanostructured polymers
ID EPOXY COMPOSITE; FATIGUE CRACKS; FRACTURE-TOUGHNESS; POLYMER NANOFIBERS;
GLASS NANOFIBERS; FIBERS; COATINGS; REPAIR; RESINS; DAMAGE
AB This article reports a novel hybrid multiscale carbon-fiber/epoxy composite reinforced with self-healing core-shell nanofibers at interfaces. The ultrathin self-healing fibers were fabricated by means of coelectrospinning, in which liquid dicyclopentadiene (DCPD) as the healing agent was enwrapped into polyacrylonitrile (PAN) to form core-shell DCPD/PAN nanofibers. These core-shell nanofibers were incorporated at interfaces of neighboring carbon-fiber fabrics prior to resin infusion and formed into ultrathin self-healing interlayers after resin infusion and curing. The core-shell DCPD/PAN fibers are expected to function to self-repair the interfacial damages in composite laminates, e.g., delamination. Wet layup, followed by vacuum-assisted resin transfer molding (VARTM) technique, was used to process the proof-of-concept hybrid multiscale self-healing composite. Three-point bending test was utilized to evaluate the self-healing effect of the core-shell nanofibers on the flexural stiffness of the composite laminate after predamage failure. Experimental results indicate that the flexural stiffness of such novel self-healing composite after predamage failure can be completely recovered by the self-healing nanofiber interlayers. Scanning electron microscope (SEM) was utilized for fractographical analysis of the failed samples. SEM micrographs clearly evidenced the release of healing agent at laminate interfaces and the toughening and self-healing mechanisms of the core-shell nanofibers. This study expects a family of novel high-strength, lightweight structural polymer composites with self-healing function for potential use in aerospace and aeronautical structures, sports utilities, etc. (c) 2012 Wiley Periodicals, Inc. J. Appl. Polym. Sci., 2013
C1 [Wu, Xiang-Fa; Rahman, Arifur; Zhou, Zhengping] N Dakota State Univ, Dept Mech Engn, Fargo, ND 58108 USA.
[Pelot, David D.; Sinha-Ray, Suman; Yarin, Alexander L.] Univ Illinois, Dept Mech & Ind Engn, Chicago, IL 60607 USA.
[Chen, Bin] NASA, Ames Res Ctr, Adv Studies Lab, Moffett Field, CA 94035 USA.
[Chen, Bin] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.
[Payne, Scott] N Dakota State Univ, Electron Microscopy Ctr, Fargo, ND 58108 USA.
RP Wu, XF (reprint author), N Dakota State Univ, Dept Mech Engn, Fargo, ND 58108 USA.
EM xiangfa.wu@ndsu.edu; ayarin@uic.edu
FU NDSU by the ND NASA EPSCoR (NASA) [NNX07AK91A, 43500-2490-FAR018640];
NDSU Development Foundation
FX The financial support of the research at NDSU by the ND NASA EPSCoR
(NASA Grant # NNX07AK91A, seed grant: 43500-2490-FAR018640) and NDSU
Development Foundation (XFW) was gratefully acknowledged. Thanks go to
Professor Chunwei Sun of the Department of Pharmacy at NDSU for kind
assistance with the optical microscopy of the core-shell nanofibers.
NR 57
TC 28
Z9 28
U1 9
U2 234
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0021-8995
J9 J APPL POLYM SCI
JI J. Appl. Polym. Sci.
PD AUG 5
PY 2013
VL 129
IS 3
BP 1383
EP 1393
DI 10.1002/app.38838
PG 11
WC Polymer Science
SC Polymer Science
GA 138JJ
UT WOS:000318504500055
ER
PT J
AU Blunden, J
Arndt, DS
Achberger, C
Ackerman, SA
Albanil, A
Alexander, P
Alfaro, EJ
Allan, R
Alves, LM
Amador, JA
Ambenje, P
Andrianjafinirina, S
Antonov, J
Aravequia, JA
Arendt, A
Arevalo, J
Ashik, I
Atheru, Z
Banzon, V
Baringer, MO
Barreira, S
Barriopedro, DE
Beard, G
Becker, A
Behrenfeld, MJ
Bell, GD
Benedetti, A
Bernhard, G
Berrisford, P
Berry, DI
Bhatt, U
Bidegain, M
Bindoff, N
Bissolli, P
Blake, ES
Booneeady, R
Bosilovich, M
Box, JE
Boyer, T
Braathen, GO
Bromwich, DH
Brown, R
Brown, L
Bruhwiler, L
Bulygina, ON
Burgess, D
Burrows, J
Calderon, B
Camargo, SJ
Campbell, J
Cao, Y
Cappelen, J
Carrasco, G
Chambers, DP
Chang'a, L
Chappell, P
Chehade, W
Cheliah, M
Christiansen, HH
Christy, JR
Ciais, P
Coelho, CAS
Cogley, JG
Colwell, S
Cross, JN
Crouch, J
Cunningham, SA
Dacic, M
De Jeu, RAM
Dekaa, FS
Demircan, M
Derksen, C
Diamond, HJ
Dlugokencky, EJ
Dohan, K
Dolman, AJ
Domingues, CM
Dong, SF
Dorigo, WA
Drozdov, DS
Duguay, CR
Dunn, RJH
Duran-Quesada, AM
Dutton, GS
Ehmann, C
Elkins, JW
Euscategui, C
Famiglietti, JS
Fang, F
Fauchereau, N
Feely, RA
Fekete, BM
Fenimore, C
Fioletov, VE
Fogarty, CT
Fogt, RL
Folland, CK
Foster, MJ
Frajka-Williams, E
Franz, BA
Frith, SH
Frolov, I
Ganter, C
Garzoli, S
Geai, ML
Gerland, S
Gitau, W
Gleason, KL
Gobron, N
Goldenberg, SB
Goni, G
Good, SA
Gottschalck, J
Gregg, MC
Griffiths, G
Grooss, JU
Guard, C
Gupta, SK
Hall, BD
Halpert, MS
Harada, Y
Hauri, C
Heidinger, AK
Heikkila, A
Heim, RR
Heimbach, P
Hidalgo, HG
Hilburn, K
Ho, SP
Hobbs, WR
Holgate
Hovsepyan, A
Hu, ZZ
Hughes, P
Hurst, DF
Ingvaldsen, R
Inness, A
Jaimes, E
Jakobsson, M
James, AI
Jeffries, MO
Johns, WE
Johnsen, B
Johnson, GC
Johnson, B
Jones, LT
Jumaux, G
Kabidi, K
Kaiser, JW
Kamga, A
Kang, KK
Kanzow, TO
Kao, HY
Keller, LM
Kennedy, JJ
Key, J
Khatiwala, S
Pour, HK
Kholodov, AL
Khoshkam, M
Kijazi, A
Kikuchi, T
Kim, BM
Kim, SJ
Kimberlain, TB
Knaff, JA
Korshunova, NN
Koskela, T
Kousky, VE
Kramarova, N
Kratz, DP
Krishfield, R
Kruger, A
Kruk, MC
Kumar, A
Lagerloef, GSE
Lakkala, K
Lander, MA
Landsea, CW
Lankhorst, M
Laurila, T
Lazzara, MA
Lee, C
Leuliette, E
Levitus, S
L'Heureux, M
Lieser, J
Lin, II
Liu, YY
Liu, Y
Liu, HX
Liu, YJ
Lobato-Sanchez, R
Locarnini, R
Loeb, NG
Loeng, H
Long, CS
Lorrey, AM
Luhunga, P
Lumpkin, R
Luo, JJ
Lyman, JM
Macdonald, AM
Maddux, BC
Malekela, C
Manney, G
Marchenko, SS
Marengo, JA
Marotzke, J
Marra, JJ
Martinez-Guingla, R
Massom, RA
Mathis, JT
McBride, C
McCarthy, G
McVicar, TR
Mears, C
Meier, W
Meinen, CS
Menendez, M
Merrifield, MA
Mitchard, E
Mitchum, GT
Montzka, SA
Morcrette, JJ
Mote, T
Muhle, J
Muhr, B
Mullan, AB
Muller, R
Nash, ER
Nerem, RS
Newlin, ML
Newman, PA
Ng'ongolo, H
Nieto, JJ
Nishino, S
Nitsche, H
Noetzli, J
Oberman, NG
Obregon, A
Ogallo, LA
Oludhe, CS
Omar, MI
Overland, J
Oyunjargal, L
Parinussa, RM
Park, GH
Park, EH
Parker, D
Pasch, RJ
Pascual-Ramirez, R
Pelto, MS
Penalba, O
Peng, L
Perovich, DK
Pezza, AB
Phillips, D
Pickart, R
Pinty, B
Pitts, MC
Purkey, SG
Quegan, S
Quintana, J
Rabe, B
Rahimzadeh, F
Raholijao, N
Raiva, I
Rajeevan, M
Ramiandrisoa, V
Ramos, A
Ranivoarissoa, S
Rayner, NA
Rayner, D
Razuveav, VN
Reagan, J
Reid, P
Renwick, J
Revedekar, J
Richter-Menge, J
Rivera, IL
Robinson, DA
Rodell, M
Romanovsky, VE
Ronchail, J
Rosenlof, KH
Sabine, CL
Salvador, MA
Sanchez-Lugo, A
Santee, ML
Sasgen, I
Sawaengphokhai, P
Sayouri, A
Scambos, TA
Schauer, U
Schemm, J
Schlosser, P
Schmid, C
Schreck, C
Semiletov, I
Send, U
Sensoy, S
Setzer, A
Severinghaus, J
Shakhova, N
Sharp, M
Shiklomanov, NI
Siegel, DA
Silva, VBS
Silva, FDS
Sima, F
Simeonov, P
Simmonds, I
Simmons, A
Skansi, M
Smeed, DA
Smethie, WM
Smith, AB
Smith, C
Smith, SL
Smith, TM
Sokolov, V
Srivastava, AK
Stackhouse PW Jr
Stammerjohn, S
Steele, M
Steffen, K
Steinbrecht, W
Stephenson, T
Su, J
Svendby, T
Sweet, W
Takahashi, T
Tanabe, RM
Taylor, MA
Tedesco, M
Teng, WL
Thepaut, JN
Thiaw, WM
Thoman, R
Thompson, P
Thorne, PW
Timmermans, ML
Tobin, S
Toole, J
Trewin, BC
Trigo, RM
Trotman, A
Tschudi, M
van de Wal, RSW
Van der Werf, GR
Vautard, R
Vazquez, JL
Vieira, G
Vincent, L
Vose, RS
Wagner, WW
Wahr, J
Walsh, J
Wang, JH
Wang, CZ
Wang, M
Wang, SH
Wang, L
Wanninkhof, R
Weaver, S
Weber, M
Werdell, PJ
Whitewood, R
Wijffels, S
Wilber, AC
Wild, JD
Willett, KM
Williams, W
Willis, JK
Wolken, G
Wong, T
Woodgate, R
Worthy, D
Wouters, B
Wovrosh, AJ
Xue, Y
Yamada, R
Yin, ZG
Yu, LS
Zhang, LY
Zhang, PQ
Zhao, L
Zhao, J
Zhong, W
Ziemke, J
Zimmermann, S
AF Blunden, Jessica
Arndt, Derek S.
Achberger, Christine
Ackerman, Stephen A.
Albanil, Adelina
Alexander, P.
Alfaro, Eric J.
Allan, Rob
Alves, Lincoln M.
Amador, Jorge A.
Ambenje, Peter
Andrianjafinirina, Solonomenjanahary
Antonov, John
Aravequia, Jose A.
Arendt, A.
Arevalo, Juan
Ashik, I.
Atheru, Zachary
Banzon, Viva
Baringer, Molly O.
Barreira, Sandra
Barriopedro, David E.
Beard, Grant
Becker, Andreas
Behrenfeld, Michael J.
Bell, Gerald D.
Benedetti, Angela
Bernhard, Germar
Berrisford, Paul
Berry, David I.
Bhatt, U.
Bidegain, Mario
Bindoff, Nathan
Bissolli, Peter
Blake, Eric S.
Booneeady, Raj
Bosilovich, Michael
Box, J. E.
Boyer, Tim
Braathen, Geir O.
Bromwich, David H.
Brown, R.
Brown, L.
Bruhwiler, Lori
Bulygina, Olga N.
Burgess, D.
Burrows, John
Calderon, Blanca
Camargo, Suzana J.
Campbell, Jayaka
Cao, Y.
Cappelen, J.
Carrasco, Gualberto
Chambers, Don P.
Chang'a, L.
Chappell, Petra
Chehade, Wissam
Cheliah, Muthuvel
Christiansen, Hanne H.
Christy, John R.
Ciais, Phillipe
Coelho, Caio A. S.
Cogley, J. G.
Colwell, Steve
Cross, J. N.
Crouch, Jake
Cunningham, Stuart A.
Dacic, Milan
De Jeu, Richard A. M.
Dekaa, Francis S.
Demircan, Mesut
Derksen, C.
Diamond, Howard J.
Dlugokencky, Ed J.
Dohan, Kathleen
Dolman, A. Johannes
Domingues, Catia M.
Dong Shenfu
Dorigo, Wouter A.
Drozdov, D. S.
Duguay, Claude R.
Dunn, Robert J. H.
Duran-Quesada, Ana M.
Dutton, Geoff S.
Ehmann, Christian
Elkins, James W.
Euscategui, Christian
Famiglietti, James S.
Fang Fan
Fauchereau, Nicolas
Feely, Richard A.
Fekete, Balazs M.
Fenimore, Chris
Fioletov, Vitali E.
Fogarty, Chris T.
Fogt, Ryan L.
Folland, Chris K.
Foster, Michael J.
Frajka-Williams, Eleanor
Franz, Bryan A.
Frith, Stacey H.
Frolov, I.
Ganter, Catherine
Garzoli, Silvia
Geai, M.-L.
Gerland, S.
Gitau, Wilson
Gleason, Karin L.
Gobron, Nadine
Goldenberg, Stanley B.
Goni, Gustavo
Good, Simon A.
Gottschalck, Jonathan
Gregg, Margarita C.
Griffiths, Georgina
Grooss, Jens-Uwe
Guard, Charles 'Chip'
Gupta, Shashi K.
Hall, Bradley D.
Halpert, Michael S.
Harada, Yayoi
Hauri, C.
Heidinger, Andrew K.
Heikkila, Anu
Heim, Richard R., Jr.
Heimbach, Patrick
Hidalgo, Hugo G.
Hilburn, Kyle
Ho, Shu-peng (Ben)
Hobbs, Will R.
Holgate, Simon
Hovsepyan, Anahit
Hu Zeng-Zhen
Hughes, P.
Hurst, Dale F.
Ingvaldsen, R.
Inness, Antje
Jaimes, Ena
Jakobsson, Martin
James, Adamu I.
Jeffries, Martin O.
Johns, William E.
Johnsen, Bjorn
Johnson, Gregory C.
Johnson, Bryan
Jones, Luke T.
Jumaux, Guillaume
Kabidi, Khadija
Kaiser, Johannes W.
Kamga, Andre
Kang, Kyun-Kuk
Kanzow, Torsten O.
Kao, Hsun-Ying
Keller, Linda M.
Kennedy, John J.
Key, J.
Khatiwala, Samar
Pour, H. Kheyrollah
Kholodov, A. L.
Khoshkam, Mahbobeh
Kijazi, Agnes
Kikuchi, T.
Kim, B.-M.
Kim, S.-J.
Kimberlain, Todd B.
Knaff, John A.
Korshunova, Natalia N.
Koskela, T.
Kousky, Vernon E.
Kramarova, Natalya
Kratz, David P.
Krishfield, R.
Kruger, Andries
Kruk, Michael C.
Kumar, Arun
Lagerloef, Gary S. E.
Lakkala, K.
Lander, Mark A.
Landsea, Chris W.
Lankhorst, Matthias
Laurila, T.
Lazzara, Matthew A.
Lee, Craig
Leuliette, Eric
Levitus, Sydney
L'Heureux, Michelle
Lieser, Jan
Lin, I-I
Liu, Y. Y.
Liu, Y.
Liu Hongxing
Liu Yanju
Lobato-Sanchez, Rene
Locarnini, Ricardo
Loeb, Norman G.
Loeng, H.
Long, Craig S.
Lorrey, Andrew M.
Luhunga, P.
Lumpkin, Rick
Luo Jing-Jia
Lyman, John M.
Macdonald, Alison M.
Maddux, Brent C.
Malekela, C.
Manney, Gloria
Marchenko, S. S.
Marengo, Jose A.
Marotzke, Jochem
Marra, John J.
Martinez-Gueingla, Rodney
Massom, Robert A.
Mathis, Jeremy T.
McBride, Charlotte
McCarthy, Gerard
McVicar, Tim R.
Mears, Carl
Meier, W.
Meinen, Christopher S.
Menendez, Melisa
Merrifield, Mark A.
Mitchard, Edward
Mitchum, Gary T.
Montzka, Stephen A.
Morcrette, Jean-Jacques
Mote, Thomas
Muehle, Jens
Muehr, Bernhard
Mullan, A. Brett
Mueller, Rolf
Nash, Eric R.
Nerem, R. Steven
Newlin, Michele L.
Newman, Paul A.
Ng'ongolo, H.
Nieto, Juan Jose
Nishino, S.
Nitsche, Helga
Noetzli, Jeannette
Oberman, N. G.
Obregon, Andre'
Ogallo, Laban A.
Oludhe, Christopher S.
Omar, Mohamed I
Overland, James
Oyunjargal, Lamjav
Parinussa, Robert M.
Park, Geun-Ha
Park, E-Hyung
Parker, David
Pasch, Richard J.
Pascual-Ramirez, Reynaldo
Pelto, Mauri S.
Penalba, Olga
Peng, L.
Perovich, Don K.
Pezza, Alexandre B.
Phillips, David
Pickart, R.
Pinty, Bernard
Pitts, Michael C.
Purkey, Sarah G.
Quegan, Shaun
Quintana, Juan
Rabe, B.
Rahimzadeh, Fatemeh
Raholijao, Nirivololona
Raiva, I.
Rajeevan, Madhavan
Ramiandrisoa, Voahanginirina
Ramos, Alexandre
Ranivoarissoa, Sahondra
Rayner, Nick A.
Rayner, Darren
Razuveav, Vyacheslav N.
Reagan, James
Reid, Phillip
Renwick, James
Revedekar, Jayashree
Richter-Menge, Jacqueline
Rivera, Ingrid L.
Robinson, David A.
Rodell, Matthew
Romanovsky, Vladimir E.
Ronchail, Josyane
Rosenlof, Karen H.
Sabine, Christopher L.
Salvador, Mozar A.
Sanchez-Lugo, Ahira
Santee, Michelle L.
Sasgen, I.
Sawaengphokhai, P.
Sayouri, Amal
Scambos, Ted A.
Schauer, U.
Schemm, Jae
Schlosser, P.
Schmid, Claudia
Schreck, Carl
Semiletov, Igor
Send, Uwe
Sensoy, Serhat
Setzer, Alberto
Severinghaus, Jeffrey
Shakhova, Natalia
Sharp, M.
Shiklomanov, Nicolai I.
Siegel, David A.
Silva, Viviane B. S.
Silva, Frabricio D. S.
Sima, Fatou
Simeonov, Petio
Simmonds, I.
Simmons, Adrian
Skansi, Maria
Smeed, David A.
Smethie, W. M.
Smith, Adam B.
Smith, Cathy
Smith, Sharon L.
Smith, Thomas M.
Sokolov, V.
Srivastava, A. K.
Stackhouse, Paul W., Jr.
Stammerjohn, Sharon
Steele, M.
Steffen, Konrad
Steinbrecht, Wolfgang
Stephenson, Tannecia
Su, J.
Svendby, T.
Sweet, William
Takahashi, Taro
Tanabe, Raymond M.
Taylor, Michael A.
Tedesco, Marco
Teng, William L.
Thepaut, Jean-Noel
Thiaw, Wassila M.
Thoman, R.
Thompson, Philip
Thorne, Peter W.
Timmermans, M.-L.
Tobin, Skie
Toole, J.
Trewin, Blair C.
Trigo, Ricardo M.
Trotman, Adrian
Tschudi, M.
van de Wal, Roderik S. W.
Van der Werf, Guido R.
Vautard, Robert
Vazquez, J. L.
Vieira, Goncalo
Vincent, Lucie
Vose, Russ S.
Wagner, Wolfgang W.
Wahr, John
Walsh, J.
Wang Junhong
Wang Chunzai
Wang, M.
Wang Sheng-Hung
Wang Lei
Wanninkhof, Rik
Weaver, Scott
Weber, Mark
Werdell, P. Jeremy
Whitewood, Robert
Wijffels, Susan
Wilber, Anne C.
Wild, J. D.
Willett, Kate M.
Williams, W.
Willis, Joshua K.
Wolken, G.
Wong, Takmeng
Woodgate, R.
Worthy, D.
Wouters, B.
Wovrosh, Alex J.
Xue Yan
Yamada, Ryuji
Yin Zungang
Yu Lisan
Zhang Liangying
Zhang Peiqun
Zhao Lin
Zhao, J.
Zhong, W.
Ziemke, Jerry
Zimmermann, S.
TI State of the Climate in 2012
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID SEA-SURFACE-TEMPERATURE; MADDEN-JULIAN OSCILLATION; WESTERN NORTH
PACIFIC; INTERNATIONAL POLAR YEAR; COUPLED KELVIN WAVES; MERIDIONAL
OVERTURNING CIRCULATION; OUTGOING LONGWAVE RADIATION; CALIFORNIA CURRENT
SYSTEM; OCEAN THERMAL STRUCTURE; GLOBAL WATER CYCLE
AB For the first time in serveral years, the El Nino-Southern Oscillation did not dominate regional climate conditions around the globe. A weak La Ni a dissipated to ENSOneutral conditions by spring, and while El Nino appeared to be emerging during summer, this phase never fully developed as sea surface temperatures in the eastern conditions. Nevertheless, other large-scale climate patterns and extreme weather events impacted various regions during the year. A negative phase of the Arctic Oscillation from mid-January to early February contributed to frigid conditions in parts of northern Africa, eastern Europe, and western Asia. A lack of rain during the 2012 wet season led to the worst drought in at least the past three decades for northeastern Brazil. Central North America also experienced one of its most severe droughts on record. The Caribbean observed a very wet dry season and it was the Sahel's wettest rainy season in 50 years.
Overall, the 2012 average temperature across global land and ocean surfaces ranked among the 10 warmest years on record. The global land surface temperature alone was also among the 10 warmest on record. In the upper atmosphere, the average stratospheric temperature was record or near-record cold, depending on the dataset. After a 30-year warming trend from 1970 to 1999 for global sea surface temperatures, the period 2000-12 had little further trend. This may be linked to the prevalence of La Ni a-like conditions during the 21st century. Heat content in the upper 700 m of the ocean remained near record high levels in 2012. Net increases from 2011 to 2012 were observed at 700-m to 2000-m depth and even in the abyssal ocean below. Following sharp decreases in to the effects of La Ni a, sea levels rebounded to reach records highs in 2012. The increased hydrological cycle seen in recent years continued, with more evaporation in drier locations and more precipitation in rainy areas. In a pattern that has held since 2004, salty areas of the ocean surfaces and subsurfaces were anomalously salty on average, while fresher areas were anomalously fresh.
Global tropical cyclone activity during 2012 was near average, with a total of 84 storms compared with the 1981-2010 average of 89. Similar to 2010 and 2011, the North Atlantic was the only hurricane basin that experienced above-normal activity. In this basin, Sandy brought devastation to Cuba and parts of the eastern North American seaboard. All other basins experienced either near-or below-normal tropical cyclone activity. Only three tropical cyclones reached Category 5 intensity-all in Bopha became the only storm in the historical record to produce winds greater than 130 kt south of 7 N. It was also the costliest storm to affect the Philippines and killed more than 1000 residents.
Minimum Arctic sea ice extent in September and Northern Hemisphere snow cover extent in June both reached new record lows. June snow cover extent is now declining at a faster rate (-17.6% per decade) than September sea ice extent (-13.0% per decade). Permafrost temperatures reached record high values in northernmost Alaska. A new melt extent record occurred on 11-12 July on the Greenland ice sheet; 97% of the ice sheet showed some form of melt, four times greater than the average melt for this time of year.
The climate in Antarctica was relatively stable overall. The largest maximum sea ice extent since records begain in 1978 was observed in September 2012. In the stratosphere, warm air led to the second smallest ozone hole in the past two decades. Even so, the springtime ozone layer above Antarctica likely will not return to its early 1980s state until about 2060.
Following a slight decline associated with the global 2 emissions from fossil fuel combustion and cement production reached a record 9.5 +/- 0.5 Pg C in 2011 and a new record of 9.7 +/- 0.5 Pg C is estimated for 2012. Atmospheric CO2 concentrations increased by 2.1 ppm in 2012, to 392.6 ppm. In spring 2012, 2 concentration exceeded 400 ppm at 7 of the 13 Arctic observation sites. Globally, other greenhouse gases including methane and nitrous oxide also continued to rise in concentration and the combined effect now represents a 32% increase in radiative forcing over a 1990 baseline. Concentrations of most ozone depleting substances continued to fall.
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[Alves, Lincoln M.] INPE, CCST, Sao Paulo, Brazil.
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[Antonov, John] Univ Corp Atmospher Res, Boulder, CO USA.
[Aravequia, Jose A.; Marchenko, S. S.] INPE, Ctr Previsao Tempo & Estudos Climat, Sao Paulo, Brazil.
[Arendt, A.; Bhatt, U.; Jeffries, Martin O.; Kholodov, A. L.; Romanovsky, Vladimir E.] Univ Alaska Fairbanks, Geophys Inst, Fairbanks, AK USA.
[Arevalo, Juan] Inst Nacl Meteorol & Hidrol Venezuela INAMEH, Caracas, Venezuela.
[Arndt, Derek S.; Banzon, Viva; Crouch, Jake; Fenimore, Chris; Gleason, Karin L.; Heim, Richard R., Jr.; Hughes, P.; Reagan, James; Sanchez-Lugo, Ahira; Smith, Adam B.; Vose, Russ S.] NOAA NESDIS Natl Climat Data Ctr, Asheville, NC USA.
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[Barreira, Sandra] Argentine Naval Hydrog Serv, Buenos Aires, DF, Argentina.
[Barriopedro, David E.] UCM, Madrid, Spain.
[Beard, Grant; Ganter, Catherine; Obregon, Andre'] Bur Meteorol, Melbourne, Vic, Australia.
[Becker, Andreas] Deutsch Wetterdienst DWD, Offenbach, Germany.
[Behrenfeld, Michael J.] Oregon State Univ, Portland, OR USA.
[Bell, Gerald D.; Gottschalck, Jonathan; Halpert, Michael S.; Hu Zeng-Zhen; Kousky, Vernon E.; Kumar, Arun; L'Heureux, Michelle; Morcrette, Jean-Jacques; Schemm, Jae; Thiaw, Wassila M.; Weaver, Scott; Wild, J. D.; Xue Yan] NOAA NWS Climate Predict Ctr, College Pk, MD USA.
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[Bernhard, Germar] Biospher Instruments, San Diego, CA USA.
[Berrisford, Paul; McCarthy, Gerard] European Ctr Medium Range Weather Forecasts, NCAS Climate, Reading, Berks, England.
[Berry, David I.; Rayner, Darren; Smeed, David A.] Natl Oceanog Ctr, Southampton, Hants, England.
[Bidegain, Mario] Direcc Nacl Meteorol, Div Climatol, Montevideo, Uruguay.
[Bindoff, Nathan] Antarctic Climate & Ecosyst Cooperat Res Ctr, Hobart, Tas, Australia.
[Bindoff, Nathan; Wijffels, Susan] CSIRO Marine & Atmospher Labs, Hobart, Tas, Australia.
[Bissolli, Peter; Pasch, Richard J.] Deutsch Wetterdienst, Offenbach, Germany.
[Blake, Eric S.; Kimberlain, Todd B.; Landsea, Chris W.] NOAA NWS Natl Hurricane Ctr, Miami, FL USA.
[Blunden, Jessica; Kruk, Michael C.; Yin Zungang] NOAA NESDIS Natl Climat Data Ctr, ERT Inc, Asheville, NC USA.
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[Bosilovich, Michael; Cheliah, Muthuvel] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD USA.
[Box, J. E.] Geol Survey Denmark & Greenland, Copenhagen, Denmark.
[Box, J. E.; Bromwich, David H.; Wang Sheng-Hung] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH USA.
[Braathen, Geir O.] WMO Atmospher Environm Res Div, Geneva, Switzerland.
[Brown, R.] Environm Canada, Climate Res Div, Montreal, PQ, Canada.
[Brown, L.; Montzka, Stephen A.] Environm Canada, Climate Res Div, Downsview, ON, Canada.
[Bruhwiler, Lori; Dlugokencky, Ed J.; Elkins, James W.; Hall, Bradley D.; Rosenlof, Karen H.] NOAA OAR Earth Syst Res Lab, Boulder, CO USA.
[Bulygina, Olga N.; Razuveav, Vyacheslav N.] Russian Inst Hydrometeorol Informat, Obninsk, Russia.
[Burgess, D.; Smith, Sharon L.] Nat Resources Canada, Geol Survey Canada, Ottawa, ON, Canada.
[Burrows, John; Takahashi, Taro] Univ Bremen, Bremen, Germany.
[Camargo, Suzana J.; Khatiwala, Samar; Schlosser, P.; Smethie, W. M.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Campbell, Jayaka; Stephenson, Tannecia; Taylor, Michael A.] Univ West Indies, Dept Phys, Kingston, Jamaica.
[Cao, Y.; Su, J.; Zhao, J.; Zhong, W.] Ocean Univ China, Qingdao, Peoples R China.
[Cappelen, J.] Danish Meteorol Inst, Copenhagen, Denmark.
[Carrasco, Gualberto] Serv Nacl Meteorol & Hidrol Bolivia SENAMHI, La Paz, Bolivia.
[Chambers, Don P.; Malekela, C.; Ng'ongolo, H.] Univ S Florida, Coll Marine Sci, St Petersburg, FL USA.
[Chang'a, L.; Kijazi, Agnes; Luhunga, P.] Tanzania Meteorol Agcy, Dar Es Salaam, Tanzania.
[Chappell, Petra; Griffiths, Georgina; Lorrey, Andrew M.; Weber, Mark] Natl Inst Water & Atmosphere Res Ltd, Auckland, New Zealand.
[Chehade, Wissam] Univ Bremen FBI, Bremen, Germany.
[Christiansen, Hanne H.] Univ Ctr Svalbard, Dept Geol, UNIS, Svalbard, Norway.
[Christiansen, Hanne H.] Univ Oslo, Dept Geosci, Oslo, Norway.
[Christy, John R.; Vautard, Robert] Univ Alabama, Huntsville, AL USA.
[Ciais, Phillipe] CEA CNR UVSQ, LSCE, Gif Sur Yvette, France.
[Coelho, Caio A. S.] CPTEC INPE Ctr Weather Forecasts & Climate Studies, Cachoeira Paulista, Brazil.
[Cogley, J. G.] Trent Univ, Dept Geog, Peterborough, ON, Canada.
[Colwell, Steve] British Antarctic Survey, Cambridge, England.
[Cross, J. N.; Hauri, C.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Fairbanks, AK USA.
[Cunningham, Stuart A.] Scottish Marine Inst Oban, Argyll, Scotland.
[Dacic, Milan; Parinussa, Robert M.] Republ Hydrometeorol Serv Serbia, Belgrade, Serbia.
[De Jeu, Richard A. M.; Dolman, A. Johannes; Van der Werf, Guido R.] Vrije Univ Amsterdam, Dept Earth Sci, Fac Earth & Life Sci, Amsterdam, Netherlands.
[Dekaa, Francis S.; James, Adamu I.; Sensoy, Serhat] Nigerian Meteorol Agency, Abuja, Nigeria.
[Demircan, Mesut] Turkish State Meteorol Serv, Ankara, Turkey.
[Derksen, C.; Worthy, D.] Environm Canada, Climate Res Div, Toronto, ON, Canada.
[Diamond, Howard J.] NOAA NESDIS Natl Climat Data Ctr, Silver Spring, MD USA.
[Dohan, Kathleen; Lagerloef, Gary S. E.] Earth & Space Res, Seattle, WA USA.
[Domingues, Catia M.] Antarctic Climate & Ecosyst Cooperat Res Ctr, Hobart, Tas, Australia.
[Dong Shenfu; Garzoli, Silvia] Cooperat Inst Marine & Atmospher Sci, Miami, FL USA.
[Dorigo, Wouter A.; Wagner, Wolfgang W.] Vienna Univ Technol, Dept Geodesy & Geoinformat, Vienna, Austria.
[Drozdov, D. S.] Earth Cryosphere Inst, Tumen, Russia.
[Duguay, Claude R.; Kang, Kyun-Kuk; Pour, H. Kheyrollah] Univ Waterloo, Interdisciplinary Ctr Climate Change, Waterloo, ON, Canada.
[Duguay, Claude R.; Kang, Kyun-Kuk; Pour, H. Kheyrollah] Univ Waterloo, Dept Geog & Environm Management, Waterloo, ON, Canada.
[Dutton, Geoff S.; Hurst, Dale F.; Wahr, John] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO USA.
[Ehmann, Christian] KIT, Inst Meteorol & Climate Res IMK, Karlsruhe, Germany.
[Euscategui, Christian] Inst Hidrol Meteorol & Estudios Ambientales, Bogota, Colombia.
[Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Fang Fan] NASA, Goddard Earth Sci Data & Informat Serv Ctr, Greenbelt, MD USA.
[Fauchereau, Nicolas] Natl Inst Water & Atmospher Res Ltd, Auckland, New Zealand.
[Fauchereau, Nicolas; Overland, James] Univ Cape Town, Dept Oceanog, Rondebosch, South Africa.
[Feely, Richard A.; Johnson, Gregory C.; Purkey, Sarah G.; Sabine, Christopher L.] NOAA OAR Pacific Marine Environ Lab, Seattle, WA USA.
[Fekete, Balazs M.] CUNY City Coll, CUNY Environm CrossRd Initiat, New York, NY USA.
[Fioletov, Vitali E.] Environm Canada, Measurements & Anal Res Sect, Toronto, ON, Canada.
[Fogarty, Chris T.] Environm Canada, Canadian Hurricane Ctr, Dartmouth, NS, Canada.
[Fogt, Ryan L.; Wovrosh, Alex J.] Ohio Univ, Dept Geog, Athens, OH USA.
[Frajka-Williams, Eleanor] Natl Oceanog Ctr, Southampton, Hants, England.
[Franz, Bryan A.; Frith, Stacey H.; Werdell, P. Jeremy; Ziemke, Jerry] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Geai, M.-L.; Sharp, M.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB, Canada.
[Gerland, S.] Norwegian Polar Res Inst, Fram Ctr, Tromso, Norway.
[Gitau, Wilson; Oludhe, Christopher S.; Pinty, Bernard] Univ Nairobi, Dept Meteorol, Nairobi, Kenya.
[Gobron, Nadine] European Commiss, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy.
Cooperat Inst Marine & Atmospher Sci, Miami, FL 33149 USA.
Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2M7, Canada.
Fram Ctr, Norwegian Polar Inst, N-9296 Tromso, Norway.
[Gupta, Shashi K.; Sawaengphokhai, P.; Wilber, Anne C.] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Harada, Yayoi] Japan Meteorol Agency, Climate Predict Div, Tokyo, Japan.
[Heikkila, Anu; Koskela, T.; Laurila, T.] Finnish Meteorol Inst, Helsinki, Finland.
[Heimbach, Patrick; Mears, Carl] MIT, Boston, MA USA.
[Hilburn, Kyle] Remote Sensing Syst, Santa Rosa, CA 95401 USA.
[Ho, Shu-peng (Ben); Muehle, Jens; Peng, L.] UCAR COSMIC, Boulder, CO USA.
[Hobbs, Will R.; Lankhorst, Matthias; Send, Uwe; Severinghaus, Jeffrey] Univ Calif San Diego, Scripps Inst Oceanography, La Jolla, CA 92093 USA.
[Hovsepyan, Anahit] Climate Res Div, Armstatehydromet, Armenia.
[Ingvaldsen, R.; Loeng, H.] Inst Marine Res, Bergen, Norway.
[Jakobsson, Martin] Stockholm Univ, Dept Geol Sci, Stockholm, Sweden.
[Johns, William E.] Rosenstiel Sch Marine & Atmospher Sci, Miami, FL USA.
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[Johnson, Bryan] NOAA OAR Earth Syst Res Lab, Global Monitoring Div, Boulder, CO USA.
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[Kabidi, Khadija; Sayouri, Amal] Direct Meteorol Natl Maroc, Rabat, Morocco.
[Kaiser, Johannes W.] Kings Coll London, London WC2R 2LS, England.
[Kaiser, Johannes W.] Max Planck Inst, Mainz, Germany.
[Kamga, Andre; Raiva, I.] African Ctr Meteorol Applicat Dev, Niamey, Niger.
[Kanzow, Torsten O.] Helmholtz Ctr Ocean Res Kiel GEOMAR, Kiel, Germany.
[Kao, Hsun-Ying] Earth & Space Res, Seattle, WA USA.
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Univ Alaska Fairbanks, Geophys Inst, Fairbanks, AK USA.
[Khoshkam, Mahbobeh; Nishino, S.] IRIMO, Tehran, Iran.
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[Lakkala, K.] Arctic Res Ctr, Finnish Meteorol Inst, Sodankyla, Finland.
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Finnish Meteorol Inst, Helsinki, Finland.
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[Lieser, Jan] Univ Tasmania, ACE CRC, Hobart, Tas, Australia.
[Lin, I-I] Natl Taiwan Univ, Taipei, Taiwan.
[Liu, Y. Y.] Univ New S Wales, Sch Civil & Environm Engn, Sydney, NSW, Australia.
[Liu Hongxing] Univ Cincinnati, Dept Geog, Cincinnati, OH USA.
[Liu Yanju] China Meteorol Adm, Natl Climate Ctr, Beijing, Peoples R China.
NASA, Langley Res Ctr, Hampton, VA USA.
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[Luo Jing-Jia; Mathis, Jeremy T.] Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia.
[Lyman, John M.; Merrifield, Mark A.] NOAA, OAR Pacific Marine Environm Lab, Seattle, WA USA.
[Lyman, John M.; Maddux, Brent C.; Thompson, Philip] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI USA.
[Maddux, Brent C.] Univ Wisconsin, AOS CIMSS, Madison, WI USA.
[Manney, Gloria] KNMI Royal Netherlands Meteorol Inst, De Bilt, Netherlands.
[Manney, Gloria] NW Res Associates Inc, Socorro, NM USA.
[Marengo, Jose A.] New Mexico Inst Min & Technol, Socorro, NM USA.
[Marotzke, Jochem] CCST, INPE, Sao Paulo, Brazil.
[Marra, John J.] Max Planck Inst Meteorol, Hamburg, Germany.
[Martinez-Gueingla, Rodney; Nieto, Juan Jose] NOAA, NESDIS Natl Climat Data Ctr, Honolulu, HI USA.
CIIFEN, Guayaquil, Ecuador.
[McVicar, Tim R.] Univ Tasmania, Australian Antarctic Div, Hobart, Tas, Australia.
[Meier, W.] CSIRO Land & Water, Canberra, ACT, Australia.
[Menendez, Melisa] Univ Colorado, Natl Snow & Ice Data Ctr, Cooperat Inst Res Environm Sci, Boulder, CO USA.
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Univ S Florida, Coll Marine Sci, St Petersburg, FL USA.
[Mote, Thomas] NOAA, OAR Earth Syst Res Lab, Boulder, CO USA.
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[Mueller, Rolf] Natl Inst Water & Atmospher Res Ltd, Wellington, New Zealand.
[Grooss, Jens-Uwe; Nerem, R. Steven] Forschungszentrum Julich, Julich, Germany.
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[Obregon, Andre'] MIREKO, Syktyvkar, Russia.
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IGAD Climate Predict & Applicat Ctr ICPAC, Nairobi, Kenya.
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[Pelto, Mauri S.] Nichols Coll, Dudley, MA USA.
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NOAA, NESDIS, Ctr Satellite Applicat & Res, College Pk, MD USA.
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[Steffen, Konrad] Swiss Fed Res Inst WSL, Birmensdorf, Switzerland.
[Steinbrecht, Wolfgang] DWD German Weather Serv, Hohenpeissenberg, Germany.
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RP Achberger, C (reprint author), Univ Gothenburg, Dept Earth Sci, Gothenburg, Sweden.
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NR 661
TC 35
Z9 36
U1 17
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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 AUG
PY 2013
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BP S1
EP S258
DI 10.1175/2013BAMSStateoftheClimate.1
PG 258
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 304EZ
UT WOS:000330731200001
ER
PT J
AU Kaber, D
Kaufmann, K
Alexander, AL
Kim, SH
Naylor, JT
Prinzel, LJ
Pankok, C
Gil, GH
AF Kaber, David
Kaufmann, Karl
Alexander, Amy L.
Kim, Sang-Hwan
Naylor, James T.
Prinzel, Lawrence J., III
Pankok, Carl, Jr.
Gil, Guk-Ho
TI Testing and Validation of a Psychophysically Defined Metric of Display
Clutter
SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS
LA English
DT Article
ID PERFORMANCE
AB Combinations of cockpit display features may lead to increased pilot perceptions of clutter. This research sought to capture pilot perceptions of display clutter associated with primary flight display features during a vertical takeoff and landing scenario and to validate a multidimensional measure of clutter previously developed for a fixed-wing environment. Sixteen active fixed-wing pilots were recruited for the study that used a simulator configured as a vertical takeoff and landing aircraft. A factor analysis was used to reduce the number of subdimensions of the clutter measure based on previous ratings data. The simplified measure revealed an increase in the number of active display features to cause an increase in perceived clutter. Displays including synthetic vision system features were perceived as significantly more cluttered than those without. Although a tunnel (highway in the sky) feature also contributed to clutter, pilots achieved higher navigation system failure detection rates when the feature was active. Significant positive correlations were found between perceived clutter and visual display properties but not between perceived clutter and performance. Although pilots rated some displays as being highly cluttered, the increased information aided navigation failure detection. Overall, the clutter measure was found to have validity and sensitivity for application across diverse flight domains.
C1 [Kaber, David; Kaufmann, Karl; Pankok, Carl, Jr.; Gil, Guk-Ho] N Carolina State Univ, Dept Ind & Syst Engn, Raleigh, NC 27695 USA.
[Alexander, Amy L.] Aptima Inc, Woburn, MA 01801 USA.
[Kim, Sang-Hwan] Univ Michigan, Dept Ind & Syst Engn, Dearborn, MI 48128 USA.
[Naylor, James T.] US Army Special Operat Command, Dept Technol Applicat Program Off, Ft Eustis, VA 23604 USA.
[Prinzel, Lawrence J., III] NASA Langley Res Ctr, Hampton, VA 23666 USA.
RP Kaber, D (reprint author), N Carolina State Univ, Dept Ind & Syst Engn, Campus Box 7906, Raleigh, NC 27695 USA.
FU NASA Langley Research Center (LaRC) [NNL06AA21A, NNX09AN72A]
FX This research was supported by NASA Langley Research Center (LaRC) under
grant numbers NNL06AA21A and NNX09AN72A. The opinions and conclusions
expressed in this paper are those of the authors and no do not
necessarily reflect the views of NASA. This research was completed while
Amy Alexander worked as a Senior Human Factors Scientist at Aptima, Inc.
We thank Emily Stelzer for participation in the planning and execution
of the flight simulator experiment. We also thank Trey Arthur and Steve
Williams for programming the Visual Imaging Simulator for Transport
Aircraft Systems computer systems to execute the flight scenario and
present all display conditions. We also thank Mike Norman for flight
mathematics to define the simulated craft trajectory and to model the
navigation system failures. Finally, we thank Randy Bailey and Steve
Young for committing NASA LaRC resources to support this project.
NR 13
TC 1
Z9 1
U1 0
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 AUG
PY 2013
VL 10
IS 8
BP 359
EP 368
DI 10.2514/1.I010048
PG 10
WC Engineering, Aerospace
SC Engineering
GA AB2GC
UT WOS:000331610200001
ER
PT J
AU Bounoua, L
Kahime, K
Houti, L
Blakey, T
Ebi, KL
Zhang, P
Imhoff, ML
Thome, KJ
Dudek, C
Sahabi, SA
Messouli, M
Makhlouf, B
El Laamrani, A
Boumezzough, A
AF Bounoua, Lahouari
Kahime, Kholoud
Houti, Leila
Blakey, Tara
Ebi, Kristie L.
Zhang, Ping
Imhoff, Marc L.
Thome, Kurtis J.
Dudek, Claire
Sahabi, Salah A.
Messouli, Mohammed
Makhlouf, Baghdad
El Laamrani, Abderrahmane
Boumezzough, Ali
TI Linking Climate to Incidence of Zoonotic Cutaneous Leishmaniasis (L.
major) in Pre-Saharan North Africa
SO INTERNATIONAL JOURNAL OF ENVIRONMENTAL RESEARCH AND PUBLIC HEALTH
LA English
DT Article
DE cutaneous leishmaniasis; surface climate indicators; incidence; climate;
NDVI; North Africa
ID PHLEBOTOMUS-PAPATASI DIPTERA; SEASONAL DISTRIBUTION; LUTZOMYIA-OVALLESI;
TEMPORAL DYNAMICS; SOUTHWEST ASIA; SAND FLIES; PSYCHODIDAE; MOROCCO;
TRANSMISSION; POPULATIONS
AB Shifts in surface climate may have changed the dynamic of zoonotic cutaneous leishmaniasis (ZCL) in the pre-Saharan zones of North Africa. Caused by Leishmania major, this form multiplies in the body of rodents serving as reservoirs of the disease. The parasite is then transmitted to human hosts by the bite of a Phlebotomine sand fly (Diptera: Psychodidae) that was previously fed by biting an infected reservoir. We examine the seasonal and interannual dynamics of the incidence of this ZCL as a function of surface climate indicators in two regions covering a large area of the semi-arid Pre-Saharan North Africa. Results suggest that in this area, changes in climate may have initiated a trophic cascade that resulted in an increase in ZCL incidence. We find the correlation between the rainy season precipitation and the same year Normalized Difference Vegetation Index (NDVI) to be strong for both regions while the number of cases of ZCL incidence lags the precipitation and NDVI by 2 years. The zoonotic cutaneous leishmaniasis seasonal dynamic appears to be controlled by minimum temperatures and presents a 2-month lag between the reported infection date and the presumed date when the infection actually occurred. The decadal increase in the number of ZCL occurrence in the region suggests that changes in climate increased minimum temperatures sufficiently and created conditions suitable for endemicity that did not previously exist. We also find that temperatures above a critical range suppress ZCL incidence by limiting the vector's reproductive activity.
C1 [Bounoua, Lahouari; Zhang, Ping; Thome, Kurtis J.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Kahime, Kholoud; Boumezzough, Ali] Cadi Ayyad Univ, Lab Ecol & Environm, Marrakech 40000, Morocco.
[Houti, Leila] Fac Med, Sidi Bel Abbes 22000, Algeria.
[Blakey, Tara] Florida Int Univ, Miami, FL 33199 USA.
[Ebi, Kristie L.] ClimAdapt LLC, Los Altos, CA 94022 USA.
[Zhang, Ping] Earth Resources Technol Inc, Laurel, MD 20707 USA.
[Imhoff, Marc L.] Pacific NW Natl Lab, Joint Global Change Res Inst, College Pk, MD 20740 USA.
[Dudek, Claire] Bethesda Chevy Chase High Sch, Bethesda, MD 20814 USA.
[Sahabi, Salah A.] Hydrometeorol Inst Training & Res, Oran 31025, Algeria.
[Messouli, Mohammed] Cadi Ayyad Univ, Lab Hydrobiol Ecotoxicol & Sanitat, Marrakech 40000, Morocco.
[Makhlouf, Baghdad] Estab Local Publ Hlth, Saida 20000, Algeria.
[El Laamrani, Abderrahmane] Minist Hlth, Directorate Epidemiol & Dis Control, Rabat 10010, Morocco.
RP Bounoua, L (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
EM Lahouari.Bounoua-1@nasa.gov; kahimkholoud@gmail.com;
leilahouti@yahoo.fr; tblakey@fiu.edu; krisebi@essllc.org;
ping.zhang@nasa.gov; marc.imhoff@pnnl.gov; kurtis.thome@nasa.gov;
cdudek@smith.edu; salah_sahabi@yahoo.com; messouli@gmail.com;
makhloufbaghdad@yahoo.fr; laamrani55@gmail.com; aboumezzough@gmail.com
FU International START Secretariat; U.S. National Science Foundation
[GEO-0627839]; IDRC-Canada (Leila Houti) [105738-001]; NASA summer
fellowships
FX This article is based on research partially supported by a sub-award
2013-01 (to Kholoud Kahime) from the International START Secretariat
with funds supplied by the U. S. Global Change Research Program
administered by the U.S. National Science Foundation under Grant Number
GEO-0627839, and by the IDRC-Canada (Leila Houti) through project#
105738-001. Tara Blakey and Claire Dudek were supported by NASA summer
fellowships. Warm thanks are due to Haj Haddou (DELM, Rabat) and Ismail
Chichaoui (SIAAP, Errachidia) for help with the epidemiological data.
NR 48
TC 11
Z9 12
U1 4
U2 12
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 1660-4601
J9 INT J ENV RES PUB HE
JI Int. J. Environ. Res. Public Health
PD AUG
PY 2013
VL 10
IS 8
BP 3172
EP 3191
DI 10.3390/ijerph10083172
PG 20
WC Environmental Sciences; Public, Environmental & Occupational Health
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health
GA 301IT
UT WOS:000330526700006
PM 23912199
ER
PT J
AU Pellegrini, A
Brizzi, A
Zhang, L
Ali, K
Hao, Y
Wu, X
Constantinou, CC
Nechayev, Y
Hall, PS
Chahat, N
Zhadobov, M
Sauleau, R
AF Pellegrini, A.
Brizzi, A.
Zhang, L.
Ali, K.
Hao, Y.
Wu, X.
Constantinou, C. C.
Nechayev, Y.
Hall, P. S.
Chahat, N.
Zhadobov, M.
Sauleau, R.
TI Antennas and Propagation for Body-Centric Wireless Communications at
Millimeter-Wave Frequencies: A Review
SO IEEE ANTENNAS AND PROPAGATION MAGAZINE
LA English
DT Article
DE Body-centric wireless communication; millimeter waves; numerical
methods; phantoms; on-body antennas
ID 60 GHZ; EQUIVALENT PHANTOM; BIOLOGICAL TISSUES; RADIO CHANNEL; BAND;
MODELS; SIMULATIONS; SURFACES; 60GHZ
AB Body-centric wireless communications represent a well-established field of research, with many studies and applications developed in a range of frequencies that extend from 400 MHz up to 10 GHz. However, many advantages can be found in operating such systems at millimeter-wave frequencies. For example, compact antennas suitable for body-centric applications can be obtained together with other benefits, such as higher data rates and reduced interference and "observability." Meanwhile, numerical modeling of antennas and propagation at millimeter-wave frequencies represents a major challenge in terms of efficiency and accuracy. The aim of this paper is to provide a review of recent progresses and outstanding challenges in the field of body-centric communication at frequencies of 60 GHz and 94 GHz.
C1 [Pellegrini, A.; Brizzi, A.; Zhang, L.; Ali, K.; Hao, Y.] Univ London, Sch Elect Engn & Comp Sci, Antennas & Electromagnet Grp, London E1 4NS, England.
[Wu, X.; Constantinou, C. C.; Nechayev, Y.; Hall, P. S.] Univ Birmingham, Sch Elect Elect & Comp Engn, Birmingham B15 2TT, W Midlands, England.
[Chahat, N.; Zhadobov, M.; Sauleau, R.] Univ Rennes 1, UMR CNRS 6164, IETR, F-35042 Rennes, France.
[Chahat, N.] CALTECH, JPL, Pasadena, CA 91109 USA.
RP Pellegrini, A (reprint author), Univ London, Sch Elect Engn & Comp Sci, Antennas & Electromagnet Grp, London E1 4NS, England.
EM alice.pellegrini@eecs.qmul.ac.uk; alessio.brizzi@eecs.qmul.ac.uk;
lianhong.zhang@eecs.qmul.ac.uk; khaleda.ali@eecs.qmul.ac.uk;
yang.hao@eecs.qmul.ac.uk; xxw881@bham.ac.uk; c.constantinou@bham.ac.uk;
yin839@bham.ac.uk; p.s.hall@bham.ac.uk; nacer.chahat@univ-rennes1.fr;
maxim.zhadobov@univ-rennes1.fr; ronan.sauleau@univ-rennes1.fr
FU EPSRC [EP/I009019/1, EP/I010491/1]; "Agence Nationale de la Recherche"
(ANR), France [ANR-09-RPDOC-003-01]; Labex CominLabs and Brittany Region
under ResCor/BoWi project; "Centre National de la Recherche Scientifique
(CNRS)," France
FX The authors thank EPSRC for providing the funding for this research
activity, under Grants EP/I009019/1 and EP/I010491/1. This work was
supported by "Agence Nationale de la Recherche" (ANR), France under
Grants ANR-09-RPDOC-003-01 (Bio-CEM project), by Labex CominLabs and
Brittany Region under ResCor/BoWi project, and by "Centre National de la
Recherche Scientifique (CNRS)," France. In addition, the authors thank
Dr. Xuesong Lu and Prof. Julian R. G. Evans for fabricating the woodpile
antenna, Dr. Akram Alomany and Prof. Clive Parini for the useful
discussions, and Prof. John Batchelor, University of Kent, for his
precious advice.
NR 82
TC 26
Z9 26
U1 0
U2 17
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1045-9243
EI 1558-4143
J9 IEEE ANTENN PROPAG M
JI IEEE Antennas Propag. Mag.
PD AUG
PY 2013
VL 55
IS 4
BP 262
EP 287
DI 10.1109/MAP.2013.6645205
PG 26
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 297EO
UT WOS:000330238500029
ER
PT J
AU Thome, K
Goldberg, M
Mita, D
Stensaas, GL
AF Thome, Kurt
Goldberg, Mitch
Mita, Dath
Stensaas, Gregory L.
CA JACIE Team
TI JACIE: A MODEL PARTNERSHIP
SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING
LA English
DT Editorial Material
C1 [Thome, Kurt] NASA, Washington, DC 20546 USA.
[Goldberg, Mitch] NOAA, Washington, DC USA.
[Mita, Dath] USDA, Washington, DC USA.
[Stensaas, Gregory L.] USGS, Garretson, SD USA.
RP Thome, K (reprint author), NASA, Washington, DC 20546 USA.
RI Thome, Kurtis/D-7251-2012
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER SOC PHOTOGRAMMETRY
PI BETHESDA
PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA
SN 0099-1112
J9 PHOTOGRAMM ENG REM S
JI Photogramm. Eng. Remote Sens.
PD AUG
PY 2013
VL 79
IS 8
BP 681
EP 682
PG 2
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
Photographic Technology
GA 295CC
UT WOS:000330093200002
ER
PT J
AU Dunagan, SE
Johnson, R
Zavaleta, J
Russell, PB
Schmid, B
Flynn, C
Redemann, J
Shinozuka, Y
Livingston, J
Segal-Rosenhaimer, M
AF Dunagan, Stephen E.
Johnson, Roy
Zavaleta, Jhony
Russell, Philip B.
Schmid, Beat
Flynn, Connor
Redemann, Jens
Shinozuka, Yohei
Livingston, John
Segal-Rosenhaimer, Michal
TI Spectrometer for Sky-Scanning Sun-Tracking Atmospheric Research (4STAR):
Instrument Technology
SO REMOTE SENSING
LA English
DT Article
DE atmosphere; climate; pollution; radiometry; technology; hyperspectral;
fiber optic
ID AEROSOL OPTICAL DEPTH; VERTICAL PROFILES; AIRBORNE; RETRIEVAL
AB The Spectrometer for Sky-Scanning, Sun-Tracking Atmospheric Research (4STAR) combines airborne sun tracking and sky scanning with diffraction spectroscopy to improve knowledge of atmospheric constituents and their links to air-pollution/climate. Direct beam hyper-spectral measurement of optical depth improves retrievals of gas constituents and determination of aerosol properties. Sky scanning enhances retrievals of aerosol type and size distribution. 4STAR measurements will tighten the closure between satellite and ground-based measurements. 4STAR incorporates a modular sun-tracking/sky-scanning optical head with fiber optic signal transmission to rack mounted spectrometers, permitting miniaturization of the external optical head, and future detector evolution. Technical challenges include compact optical collector design, radiometric dynamic range and stability, and broad spectral coverage. Test results establishing the performance of the instrument against the full range of operational requirements are presented, along with calibration, engineering flight test, and scientific field campaign data and results.
C1 [Dunagan, Stephen E.; Johnson, Roy; Zavaleta, Jhony; Russell, Philip B.; Redemann, Jens; Segal-Rosenhaimer, Michal] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Schmid, Beat; Flynn, Connor] Pacific NW Natl Lab, Richland, WA 99325 USA.
[Shinozuka, Yohei] NASA, Ames Cooperat Res Earth Sci & Technol ARC CREST, Moffett Field, CA 94035 USA.
[Shinozuka, Yohei] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Livingston, John] SRI Int, Menlo Pk, CA 94025 USA.
RP Dunagan, SE (reprint author), NASA, Ames Res Ctr, MS 245-4, Moffett Field, CA 94035 USA.
EM Stephen.E.Dunagan@nasa.gov; Roy.R.Johnson@nasa.gov;
Jhony.R.Zavaleta@nasa.gov; Philip.B.Russell@nasa.gov;
beat.schmid@pnnl.gov; connor.flynn@pnnl.gov; Jens.Redemann-1@nasa.gov;
Yohei.Shinozuka@nasa.gov; John.M.Livingston@nasa.gov;
Michal.Segalrozenhaimer@nasa.gov
FU NASA Radiation Science Program; Ames Instrument Working Group; DOE
Atmospheric Radiation Measurement Program, Battelle's Pacific Northwest
Division; NOAA Office of Global Programs
FX 4STAR design, development, and testing were supported by the NASA
Radiation Science Program, the Ames Instrument Working Group, the DOE
Atmospheric Radiation Measurement Program, Battelle's Pacific Northwest
Division, and the NOAA Office of Global Programs. Instrument conceptual
advice and scientific data analysis software were provided by the NASA
Goddard AERONET group under the leadership of Brent Holben.
NR 18
TC 10
Z9 10
U1 0
U2 8
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD AUG
PY 2013
VL 5
IS 8
BP 3872
EP 3895
DI 10.3390/rs5083872
PG 24
WC Remote Sensing
SC Remote Sensing
GA 274SI
UT WOS:000328626100011
ER
PT J
AU Zeng, FW
Collatz, GJ
Pinzon, JE
Ivanoff, A
AF Zeng, Fan-Wei
Collatz, G. James
Pinzon, Jorge E.
Ivanoff, Alvaro
TI Evaluating and Quantifying the Climate-Driven Interannual Variability in
Global Inventory Modeling and Mapping Studies (GIMMS) Normalized
Difference Vegetation Index (NDVI3g) at Global Scales
SO REMOTE SENSING
LA English
DT Article
DE GIMMS NDVI3g; climate-driven interannual variability; interference
ID TIME-SERIES; ATMOSPHERIC CO2; ECOSYSTEM PRODUCTION; PRIMARY
PRODUCTIVITY; SURFACE-TEMPERATURE; GREAT-PLAINS; PART I; LAND;
PRECIPITATION; SATELLITE
AB Satellite observations of surface reflected solar radiation contain information about variability in the absorption of solar radiation by vegetation. Understanding the causes of variability is important for models that use these data to drive land surface fluxes or for benchmarking prognostic vegetation models. Here we evaluated the interannual variability in the new 30.5-year long global satellite-derived surface reflectance index data, Global Inventory Modeling and Mapping Studies normalized difference vegetation index (GIMMS NDVI3g). Pearson's correlation and multiple linear stepwise regression analyses were applied to quantify the NDVI interannual variability driven by climate anomalies, and to evaluate the effects of potential interference (snow, aerosols and clouds) on the NDVI signal. We found ecologically plausible strong controls on NDVI variability by antecedent precipitation and current monthly temperature with distinct spatial patterns. Precipitation correlations were strongest for temperate to tropical water limited herbaceous systems where in some regions and seasons > 40% of the NDVI variance could be explained by precipitation anomalies. Temperature correlations were strongest in northern mid- to high-latitudes in the spring and early summer where up to 70% of the NDVI variance was explained by temperature anomalies. We find that, in western and central North America, winter-spring precipitation determines early summer growth while more recent precipitation controls NDVI variability in late summer. In contrast, current or prior wet season precipitation anomalies were correlated with all months of NDVI in sub-tropical herbaceous vegetation. Snow, aerosols and clouds as well as unexplained phenomena still account for part of the NDVI variance despite corrections. Nevertheless, this study demonstrates that GIMMS NDVI3g represents real responses of vegetation to climate variability that are useful for global models.
C1 [Zeng, Fan-Wei; Pinzon, Jorge E.] NASA, SSAI, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Collatz, G. James] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ivanoff, Alvaro] NASA, ADNET, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zeng, FW (reprint author), NASA, SSAI, Biospher Sci Lab, Goddard Space Flight Ctr, Code 618, Greenbelt, MD 20771 USA.
EM fanwei.zeng@nasa.gov; george.j.collatz@nasa.gov;
jorge.e.pinzon@nasa.gov; alvaro.ivanoff@nasa.gov
RI collatz, george/D-5381-2012
FU NASA [NNH10ZDA001N-CARBON, NNH09ZDA001N-ACOS]
FX This work was supported by NASA grants NNH10ZDA001N-CARBON, Carbon
Monitoring System, and NNH09ZDA001N-ACOS. We acknowledge Douglas C.
Morton, Bin Tan, and Koen Hufkens for their assistance in phenology data
acquisition and processing. We thank Sietse O. Los for his feedbacks to
this manuscript. We also acknowledge Zheng Li for contributions early on
in this study.
NR 71
TC 40
Z9 46
U1 0
U2 29
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD AUG
PY 2013
VL 5
IS 8
BP 3918
EP 3950
DI 10.3390/rs5083918
PG 33
WC Remote Sensing
SC Remote Sensing
GA 274SI
UT WOS:000328626100013
ER
PT J
AU Cook, BD
Corp, LA
Nelson, RF
Middleton, EM
Morton, DC
McCorkel, JT
Masek, JG
Ranson, KJ
Ly, V
Montesano, PM
AF Cook, Bruce D.
Corp, Lawrence A.
Nelson, Ross F.
Middleton, Elizabeth M.
Morton, Douglas C.
McCorkel, Joel T.
Masek, Jeffrey G.
Ranson, Kenneth J.
Vuong Ly
Montesano, Paul M.
TI NASA Goddard's LiDAR, Hyperspectral and Thermal (G-LiHT) Airborne Imager
SO REMOTE SENSING
LA English
DT Article
DE remote sensing; airborne scanning LiDAR; imaging spectroscopy; surface
temperature; sensor fusion; data fusion; ecosystem structure; forest
disturbance; forest health; primary production
ID CARBON; EFFICIENCY
AB The combination of LiDAR and optical remotely sensed data provides unique information about ecosystem structure and function. Here, we describe the development, validation and application of a new airborne system that integrates commercial off the shelf LiDAR hyperspectral and thermal components in a compact, lightweight and portable system. Goddard's LiDAR, Hyperspectral and Thermal (G-LiHT) airborne imager is a unique system that permits simultaneous measurements of vegetation structure, foliar spectra and surface temperatures at very high spatial resolution (approximate to 1 m) on a wide range of airborne platforms. The complementary nature of LiDAR, optical and thermal data provide an analytical framework for the development of new algorithms to map plant species composition, plant functional types, biodiversity, biomass and carbon stocks, and plant growth. In addition, G-LiHT data enhance our ability to validate data from existing satellite missions and support NASA Earth Science research. G-LiHT's data processing and distribution system is designed to give scientists open access to both low- and high-level data products (http://gliht.gsfc.nasa.gov), which will stimulate the community development of synergistic data fusion algorithms. G-LiHT has been used to collect more than 6,500 km(2) of data for NASA-sponsored studies across a broad range of ecoregions in the USA and Mexico. In this paper, we document G-LiHT design considerations, physical specifications, instrument performance and calibration and acquisition parameters. In addition, we describe the data processing system and higher-level data products that are freely distributed under NASA's Data and Information policy.
C1 [Cook, Bruce D.; Nelson, Ross F.; Middleton, Elizabeth M.; Morton, Douglas C.; McCorkel, Joel T.; Masek, Jeffrey G.; Ranson, Kenneth J.; Vuong Ly] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Corp, Lawrence A.; Montesano, Paul M.] Sigma Space Corp, Lanham, MD 20706 USA.
RP Cook, BD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM bruce.cook@nasa.gov; lawrence.a.corp@nasa.gov; ross.f.nelson@nasa.gov;
elizabeth.m.middleton@nasa.gov; douglas.morton@nasa.gov;
joel.mccorkel@nasa.gov; jeffrey.g.masek@nasa.gov;
kenneth.j.ranson@nasa.gov; vuong.t.ly@nasa.gov;
paul.m.montesano@nasa.gov
RI Morton, Douglas/D-5044-2012; Masek, Jeffrey/D-7673-2012; McCorkel,
Joel/D-4454-2012; Ranson, Kenneth/G-2446-2012; Nelson, Ross/H-8266-2014
OI McCorkel, Joel/0000-0003-2853-2036; Ranson, Kenneth/0000-0003-3806-7270;
FU NASA Goddard Space Flight Center's Internal Research and Development
program; NASA's Terrestrial Ecology, Carbon Cycle and Carbon Monitoring
System programs
FX This research was funded in part by NASA Goddard Space Flight Center's
Internal Research and Development program and NASA's Terrestrial
Ecology, Carbon Cycle and Carbon Monitoring System programs. The authors
wish to thank NASA Langley Research Center, who provided engineering and
aircraft support throughout this project, Riegl USA and Headwall
Photonics, who provided technical assistance with instrument
installation and testing, and Timothy Creech and Joshua Bronston for
their participation in the development of GCAP.
NR 26
TC 48
Z9 50
U1 4
U2 39
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD AUG
PY 2013
VL 5
IS 8
BP 4045
EP 4066
DI 10.3390/rs5084045
PG 22
WC Remote Sensing
SC Remote Sensing
GA 274SI
UT WOS:000328626100018
ER
PT J
AU Albergel, C
Dorigo, W
Reichle, RH
Balsamo, G
de Rosnay, P
Munoz-Sabater, J
Isaksen, L
de Jeu, R
Wagner, W
AF Albergel, C.
Dorigo, W.
Reichle, R. H.
Balsamo, G.
de Rosnay, P.
Munoz-Sabater, J.
Isaksen, L.
de Jeu, R.
Wagner, W.
TI Skill and Global Trend Analysis of Soil Moisture from Reanalyses and
Microwave Remote Sensing
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Hydrometeorology; Model evaluation; performance; Reanalysis data
ID IN-SITU OBSERVATIONS; LAND-SURFACE SCHEME; SOUTHWESTERN FRANCE;
VALIDATION; SATELLITE; RETRIEVALS; PRODUCTS; ASCAT; PERFORMANCE; NETWORK
AB In situ soil moisture measurements from 2007 to 2010 for 196 stations from five networks across the world (United States, France, Spain, China, and Australia) are used to determine the reliability of three soil moisture products: (i) a revised version of the ECMWF Interim Re-Analysis (ERA-Interim; ERA-Land); (ii) a revised version of the Modern-Era Retrospective Analysis for Research and Applications (MERRA) reanalysis from NASA (MERRA-Land); and (iii) a new, microwave-based multisatellite surface soil moisture dataset (SM-MW). Evaluation of the time series and anomalies from a moving monthly mean shows a good performance of the three products in capturing the annual cycle of surface soil moisture and its short-term variability. On average, correlations (95% confidence interval) are 0.66 (+/- 0.038), 0.69 (+/- 0.038), and 0.60 (+/- 0.061) for ERA-Land, MERRA-Land, and SM-MW. The two reanalysis products also capture the root-zone soil moisture well; on average, correlations are 0.68 (+/- 0.035) and 0.73 (+/- 0.032) for ERA-Land and MERRA-Land, respectively. Global trends analysis for 1988-2010 suggests a decrease of surface soil moisture contents (72% of significant trends are negative, i.e., drying) for ERA-Land and an increase in surface soil moisture (59% of significant trends are positive, i.e., wetting) for MERRA-Land. As the spatial extent and fractions of significant trends in both products differ, the trend reflected in the majority of grid points within different climate classes was investigated and compared to that of SM-MW. The latter is dominated by negative significant trends (73.2%) and is more in line with ERA-Land. For both reanalysis products, trends for the upper layer of soil are confirmed in the root-zone soil moisture (first meter of soil).
C1 [Albergel, C.; Balsamo, G.; de Rosnay, P.; Munoz-Sabater, J.; Isaksen, L.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[Dorigo, W.; Wagner, W.] Vienna Univ Technol, Dept Geodesy & Geoinformat, A-1040 Vienna, Austria.
[Reichle, R. H.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[de Jeu, R.] Vrije Univ Amsterdam, Fac Earth & Life Sci, Dept Earth Sci, Amsterdam, Netherlands.
RP Albergel, C (reprint author), European Ctr Medium Range Weather Forecasts, Shinfield Pk, Reading RG2 9AX, Berks, England.
EM clement.albergel@ecmwf.int
RI de Rosnay, Patricia/M-8203-2013; Reichle, Rolf/E-1419-2012;
OI de Rosnay, Patricia/0000-0002-7374-3820; Dorigo,
Wouter/0000-0001-8054-7572; Balsamo, Gianpaolo/0000-0002-1745-3634;
Albergel, Clement/0000-0003-1095-2702; Wagner,
Wolfgang/0000-0001-7704-6857
FU ARC [DP0343778, DP0557543]; EUMETSAT Satellite Application Facility on
Support to Operational Hydrology and Water Management (HSAF); ESA
Climate Change Initiative (CCI); NASA
FX The authors would like to acknowledge J.-C. Calvet from Meteo-France for
giving us access to the SMOSMANIA data. J. Walker and C. Rudiger from
Monash University are thanked for the OzNet soil moisture data. The
initial setup and maintenance of the OzNet monitoring network were
funded by two ARC grants (DP0343778 and DP0557543). Thanks to D. Dee and
P. Poli from the reanalysis section of ECMWF for the fruitful
discussion. R. Riddaway from ECMWF is thanked for his valuable comments
on the English style. A. Bowen and R. Hines from ECMWF are thanked for
their help in improving the figures. The authors thank the EUMETSAT
Satellite Application Facility on Support to Operational Hydrology and
Water Management (HSAF) and the ESA Climate Change Initiative (CCI) for
their funding support. Rolf Reichle was supported by the NASA program on
The Science of Terra and Aqua. MERRA-Land data are generated using
resources provided by the NASA High-End Computing program.
NR 65
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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 AUG
PY 2013
VL 14
IS 4
BP 1259
EP 1277
DI 10.1175/JHM-D-12-0161.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 240FC
UT WOS:000326079300014
ER
PT J
AU Ozsoy-Cicek, B
Ackley, S
Xie, HJ
Yi, DH
Zwally, J
AF Ozsoy-Cicek, Burcu
Ackley, Stephen
Xie, Hongjie
Yi, Donghui
Zwally, Jay
TI Sea ice thickness retrieval algorithms based on in situ surface
elevation and thickness values for application to altimetry
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE sea ice thickness; snow depth; snow elevation; Antarctica; buoyancy
theorem
ID WESTERN WEDDELL-SEA; SNOW-DEPTH; AMSR-E; EAST ANTARCTICA; SATELLITE;
FREEBOARD; SUMMER; WINTER; FLUX; OCEAN
AB In situ measurements of sea ice thickness (I), snow depth (S), and snow freeboard (F-sn) from drilling profile lines from 15 cruises into the Southern Ocean, Antarctica, were analyzed. I was calculated from in situ F-sn and S using an isostatic approach. I was also directly estimated from F-sn as can be obtained from laser altimetry. The root-mean-square difference (RMSD) between observed and calculated I reduces, and the correlation between F-sn and I increases substantially, when (1) using values averaged over the survey lines (approximate to 50 m) instead of single drill hole measurements (approximate to 1 m) and (2) treating positive and negative sea ice freeboard (F-i) separately. For small F-i, however, S approximates F-sn pointing toward an isostatic balance also between S and I. Our linear regression analysis between the in situ measurements suggests a direct conversion of F-sn into I using a region-specific set of equations. RMSD values are similar to those obtained employing isostatic balance models and treating positive and negative F-i separately. However, more data would have been needed to obtain significant differences between most of the various models suggested. Still our new approach gives a viable alternative for Antarctic I retrieval from altimetric measurements of F-sn alone. Correlation between in situ observations of F-sn and S is high. RMSD between observed and calculated S is small. This suggests estimation of S from altimetric F-sn measurements. Such S has an estimated precision of approximate to 5 cm, and is neither affected by snow wetness or grain size nor limited to S<50 cm.
C1 [Ozsoy-Cicek, Burcu] Istanbul Tech Univ, Maritime Fac, TR-80626 Istanbul, Turkey.
[Ackley, Stephen; Xie, Hongjie] Univ Texas San Antonio, Dept Geol Sci, Lab Remote Sensing & Geoinformat, San Antonio, TX USA.
[Yi, Donghui; Zwally, Jay] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
RP Ozsoy-Cicek, B (reprint author), Istanbul Tech Univ, Maritime Fac, MaRS Maritime Remote Sensing Lab, TR-34940 Tuzla Ist, Turkey.
EM ozsoybu@itu.edu.tr
RI Xie, Hongjie/B-5845-2009
OI Xie, Hongjie/0000-0003-3516-1210
FU United States National Science Foundation (NSF) grant ANT [AWT0703682];
NASA grant [NNX08AQ87G]
FX We dedicate this paper in memory of our colleague and friend, Seymour
Laxon, who pioneered in the application of satellite altimetry to the
measurement of sea ice thickness. We would like to acknowledge the
scientists for their effort in conducting snow and ice thickness
measurements for each cruise. We also would like to acknowledge
captains, the officers, and crews who provided successful cruises. We
want to thank the AADC (http://data.aad.gov.au/) for providing data. We
wish to acknowledge United States National Science Foundation (NSF)
grant ANT (AWT0703682) and NASA grant (NNX08AQ87G) to UTSA for support.
We wish to acknowledge Stefan Kern and Cathleen Geiger for contributing
with valuable discussions and two anonymous reviewers for their
constructive comments and suggestions that greatly improved the paper.
NR 52
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U1 2
U2 17
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 AUG
PY 2013
VL 118
IS 8
BP 3807
EP 3822
DI 10.1002/jgrc.20252
PG 16
WC Oceanography
SC Oceanography
GA 224XX
UT WOS:000324927000006
ER
PT J
AU Lemoine, FG
Goossens, S
Sabaka, TJ
Nicholas, JB
Mazarico, E
Rowlands, DD
Loomis, BD
Chinn, DS
Caprette, DS
Neumann, GA
Smith, DE
Zuber, MT
AF Lemoine, Frank G.
Goossens, Sander
Sabaka, Terence J.
Nicholas, Joseph B.
Mazarico, Erwan
Rowlands, David D.
Loomis, Bryant D.
Chinn, Douglas S.
Caprette, Douglas S.
Neumann, Gregory A.
Smith, David E.
Zuber, Maria T.
TI High- degree gravity models from GRAIL primary mission data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE lunar gravity; orbit determination; KBRR data; planetary geodesy
ID LUNAR RECONNAISSANCE ORBITER; SPACE-TIME FRAME; TRACKING DATA;
COORDINATE TIME; RADIO TRACKING; PROPER TIME; FIELD; MOON; SYSTEM; EARTH
AB We have analyzed Kaband range rate (KBRR) and Deep Space Network (DSN) data from the Gravity Recovery and Interior Laboratory (GRAIL) primary mission (1 March to 29 May 2012) to derive gravity models of the Moon to degree 420, 540, and 660 in spherical harmonics. For these models, GRGM420A, GRGM540A, and GRGM660PRIM, a Kaula constraint was applied only beyond degree 330. Variancecomponent estimation (VCE) was used to adjust the a priori weights and obtain a calibrated error covariance. The global rootmeansquare error in the gravity anomalies computed from the error covariance to 320x320 is 0.77 mGal, compared to 29.0 mGal with the preGRAIL model derived with the SELENE mission data, SGM150J, only to 140x140. The global correlations with the Lunar Orbiter Laser Altimeterderived topography are larger than 0.985 between =120 and 330. The freeair gravity anomalies, especially over the lunar farside, display a dramatic increase in detail compared to the preGRAIL models (SGM150J and LP150Q) and, through degree 320, are free of the orbittrackrelated artifacts present in the earlier models. For GRAIL, we obtain an a posteriori fit to the Sband DSN data of 0.13 mm/s. The a posteriori fits to the KBRR data range from 0.08 to 1.5 m/s for GRGM420A and from 0.03 to 0.06 m/s for GRGM660PRIM. Using the GRAIL data, we obtain solutions for the degree 2 Love numbers, k(20)=0.0246150.0000914, k(21)=0.0239150.0000132, and k(22)=0.0248520.0000167, and a preliminary solution for the k(30) Love number of k(30)=0.007340.0015, where the Love number error sigmas are those obtained with VCE.
Key Points
Analyze satellite-to-satellite and DSN data to the GRAIL spacecraft Determine gravity field solutions to 660x660 in spherical harmonics Use variance component estimation to calibrate solution errors
C1 [Lemoine, Frank G.; Goossens, Sander; Sabaka, Terence J.; Nicholas, Joseph B.; Mazarico, Erwan; Rowlands, David D.; Loomis, Bryant D.; Chinn, Douglas S.; Caprette, Douglas S.; Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Goossens, Sander] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21228 USA.
[Nicholas, Joseph B.] Emergent Space Technol, Greenbelt, MD USA.
[Mazarico, Erwan; Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA.
[Loomis, Bryant D.; Chinn, Douglas S.; Caprette, Douglas S.] Stinger Ghaffarian Technol Inc, Greenbelt, MD USA.
RP Lemoine, FG (reprint author), Code 698 NASA Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
EM Frank.G.Lemoine@nasa.gov
RI Neumann, Gregory/I-5591-2013; Lemoine, Frank/D-1215-2013; Mazarico,
Erwan/N-6034-2014; Rowlands, David/D-2751-2012; Goossens,
Sander/K-2526-2015
OI Neumann, Gregory/0000-0003-0644-9944; Mazarico,
Erwan/0000-0003-3456-427X; Goossens, Sander/0000-0002-7707-1128
FU NASA Center for Climate Simulation (NCCS) at the NASA Goddard Space
Flight Center; NASA GRAIL Mission; NASA Discovery Program
FX We acknowledge the GRAIL Level 1B data team at the Jet Propulsion
Laboratory (JPL) led by Gerhard Kruizinga for their production of the
KBRR data. The high-degree GRAIL geopotential solutions were produced
using the supercomputers at the NASA Center for Climate Simulation
(NCCS) at the NASA Goddard Space Flight Center, and we acknowledge their
support. Despina E. Pavlis (SGT Inc. and NASA GSFC) supported the
upgrade of GEODYN to handle the DSN and KBRR tracking data from GRAIL.
Our localized spherical harmonic analyses and associated Legendre
polynomial evaluation tests made use of the freely available software
archive SHTOOLS (http://shtools.ipgp.fr). The Generic Mapping Tools
(GMT) package was used to produce some of the figures in this paper
[Wessel and Smith, 1998]. This work was supported by the NASA GRAIL
Mission under the auspices of the NASA Discovery Program.
NR 79
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U1 0
U2 16
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD AUG
PY 2013
VL 118
IS 8
BP 1676
EP 1698
DI 10.1002/jgre.20118
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 226AR
UT WOS:000325007100006
ER
PT J
AU Marshall, ST
Funning, GJ
Owen, SE
AF Marshall, Scott T.
Funning, Gareth J.
Owen, Susan E.
TI Fault slip rates and interseismic deformation in the western Transverse
Ranges, California
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Review
DE interseismic deformation; Transverse Ranges; strain inversion;
mechanical model; dislocation model; fault slip rate
ID SAN-ANDREAS-FAULT; LOS-ANGELES BASIN; TECTONIC BOUNDARY-CONDITIONS; 1994
NORTHRIDGE EARTHQUAKES; NEOGENE CRUSTAL ROTATIONS; RECENT SURFACE
RUPTURE; BLIND-THRUST SYSTEM; OAK-RIDGE FAULT; SOUTHERN-CALIFORNIA;
VENTURA BASIN
AB To better constrain fault slip rates and patterns of interseismic deformation in the western Transverse Ranges of southern California, we present results from analysis of GPS and interferometric synthetic aperture radar (InSAR) data and three-dimensional mechanical and kinematic models of active faulting. Anthropogenic motions are detected in several localized zones but do not significantly affect the vast majority of continuous GPS site locations. GPS measures contraction rates across the Ventura Basin of similar to 7 mm/yr oriented west-northwest with rates decreasing to the west and east. The Santa Barbara channel is accommodating similar to 6.5 mm/yr in the east and similar to 2.5 mm/yr in the western portions of N/S contraction. Inversion of horizontal GPS velocities highlights a zone of localized fast contraction rates following the Ventura Basin. Using a mechanical model driven by geodetically calculated strain rates, we show that there are no significant discrepancies between short-term slip rates captured by geodesy and longer-term slip rates measured by geology. Mechanical models reproduce the first-order interseismic velocity and strain rate patterns but fail to reproduce strongly localized contraction in the Ventura Basin due to the inadequate homogeneous elastic properties of the model. Existing two-dimensional models match horizontal rates but predict significant uplift gradients that are not observed in the GPS data. Mechanical models predict zones of fast contraction in the Santa Barbara channel and offshore near Malibu, suggesting that offshore faults represent a significant seismic hazard to the region. Furthermore, many active faults throughout the region may produce little to no interseismic deformation, making accurate seismic hazard assessment challenging.
C1 [Marshall, Scott T.] Appalachian State Univ, Dept Geol, Boone, NC 28608 USA.
[Funning, Gareth J.] Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA.
[Owen, Susan E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Marshall, ST (reprint author), Appalachian State Univ, Dept Geol, 572 Rivers St, Boone, NC 28608 USA.
EM marshallst@appstate.edu
OI Funning, Gareth/0000-0002-8247-0545
FU Southern California Earthquake Center; NSF [EAR-0529922]; USGS
[07HQAG0008]
FX This work benefitted from constructive reviews from two anonymous
reviewers. All figures were made with Generic Mapping Tools [Wessel and
Smith, 1998]. Focused SAR images were produced using the ROI_PAC
software package developed by the Jet Propulsion Laboratory.
Interferograms were formed using the DORIS software package developed by
the Delft University of Technology. The StaMPS software package was
provided by Delft University. Envisat data was provided by UNAVCO and
the WINSAR consortium. The MEaSUREs GPS time series data and the QOCA
software package were provided by the Jet Propulsion Laboratory. This
research was supported by the Southern California Earthquake Center.
SCEC is funded by NSF Cooperative Agreement EAR-0529922 and USGS
Cooperative Agreement 07HQAG0008. The SCEC contribution number for this
paper is 1744.
NR 107
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U1 0
U2 16
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 AUG
PY 2013
VL 118
IS 8
BP 4511
EP 4534
DI 10.1002/jgrb.50312
PG 24
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 225VH
UT WOS:000324991900040
ER
PT J
AU Xie, H
St Cyr, OC
Gopalswamy, N
Odstrcil, D
Cremades, H
AF Xie, H.
St Cyr, O. C.
Gopalswamy, N.
Odstrcil, D.
Cremades, H.
TI Understanding shock dynamics in the inner heliosphere with modeling and
type II radio data: A statistical study
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE coronal mass ejection; interplanetary shock; ENLIL model; type II burst
ID CORONAL MASS EJECTIONS; ENERGETIC PARTICLE EVENTS; SOLAR-WIND;
INTERPLANETARY SHOCKS; STEREO MISSION; SPACE WEATHER; PROPAGATION; CMES
AB We study two methods of predicting interplanetary shock location and strength in the inner heliosphere: (1) the ENLIL simulation and (2) the kilometric type II (kmTII) prediction. To evaluate differences in the performance of the first method, we apply two sets of coronal mass ejections (CME) parameters from the cone-model fitting and flux-rope (FR) model fitting as input to the ENLIL model for 16 halo CMEs. The results show that the ENLIL model using the actual CME speeds from FR-fit provided an improved shock arrival time (SAT) prediction. The mean prediction errors for the FR and cone-model inputs are 4.905.92 h and 5.486.11 h, respectively. A deviation of 100 km s(-1) from the actual CME speed has resulted in a SAT error of 3.46 h on average. The simulations show that the shock dynamics in the inner heliosphere agrees with the drag-based model. The shock acceleration can be divided as two phases: a faster deceleration phase within 50 R-s and a slower deceleration phase at distances beyond 50 R-s. The linear-fit deceleration in phase 1 is about 1 order of magnitude larger than that in phase 2. When applying the kmTII method to 14 DH-km CMEs, we found that combining the kmTII method with the ENLIL outputs improved the kmTII prediction. Due to a better modeling of plasma density upstream of shocks and the kmTII location, we are able to provide a more accurate shock time-distance and speed profiles. The mean kmTII prediction error using the ENLIL model density is 6.76.4 h; it is 8.410.4 h when the average solar wind plasma density is used. Applying the ENLIL density has reduced the mean kmTII prediction error by approximate to 2 h and the standard deviation by 4.0 h. Especially when we applied the combined approach to two interacting events, the kmTII prediction error was drastically reduced from 29.6 h to -4.9 h in one case and 10.6 h to 4.2 h in the other. Furthermore, the results derived from the kmTII method and the ENLIL simulation, together with white-light data, provide a valuable validation of shock formation location and strength. Such information has important implications for solar energetic particle acceleration.
C1 [Xie, H.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Xie, H.; St Cyr, O. C.; Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Odstrcil, D.] George Mason Univ, Dept Computat & Data Sci, Fairfax, VA 22030 USA.
[Cremades, H.] UTN FRM, CONICET, Mendoza, Argentina.
RP Xie, H (reprint author), Catholic Univ Amer, Dept Phys, 200 Hannan Hall, Washington, DC 20064 USA.
EM hong.xie@nasa.gov
OI Gopalswamy, Nat/0000-0001-5894-9954
FU STEREO team; SOHO team; WIND team; ACE team; NASA LWS TRT program
[08-LWSTRT08-0029]
FX The authors would like to thank the support of the STEREO, SOHO, WIND,
and ACE teams. The STEREO SECCHI data are produced by a consortium of
RAL (UK), NRL (USA), LMSAL (USA), GSFC (USA), MPS (Germany), CSL
(Belgium), IOTA (France), and IAS (France). The SOHO LASCO data are
produced by a consortium of the Naval Research Laboratory (USA),
Max-Planck-Institut fRur Aeronomie (Germany), Laboratoire d'Astronomie
(France), and the University of Birmingham (UK). We acknowledge
magnetogram data from NSO/GONG (Global Oscillation Network Group) and
the WIND data from NASA's Space Physics Data Facility. This work was
supported by NASA LWS TR&T program (08-LWSTRT08-0029). H.C. is a member
of Carrera del Investigador Cientifico, CONICET.
NR 39
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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 AUG
PY 2013
VL 118
IS 8
BP 4711
EP 4723
DI 10.1002/jgra.50444
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 225VK
UT WOS:000324992300001
ER
PT J
AU Broiles, TW
Desai, MI
Lee, CO
MacNeice, PJ
AF Broiles, T. W.
Desai, M. I.
Lee, C. O.
MacNeice, P. J.
TI Radial evolution of the three-dimensional structure in CIRs between
Earth and Ulysses
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE CIR; Enlil; magnetic field; planar magnetic structure
ID COROTATING INTERACTION REGIONS; ADVANCED COMPOSITION EXPLORER; PLANAR
MAGNETIC-STRUCTURES; SOLAR-WIND; LATITUDINAL VARIATION; TRANSPORT;
MISSION; AU
AB The radial alignment of ACE and Ulysses in February 2004 and August 2007 provided us with unprecedented opportunities to study the radial evolution of planar magnetic structures (PMSs) in three corotating interaction regions (CIRs). The in situ observations are compared with results from an analytical and a numerical model of CIRs. We find that (1) all three CIRs' meridional tilt retained its North/South orientation at ACE and Ulysses, but the evolution was not systematic. Further, the model results of CIR meridional tilt do not agree with observations. (2) All three CIRs rotated azimuthally with the Parker spiral as expected; however, model results only describe this behavior quantitatively for one CIR. (3) For all three CIRs, the solar wind deflection angles were predicted by the coupled solar corona-solar wind models, Wang-Sheely-Arge (WSA)-Enlil and MHD Around a Sphere (MAS)-Enlil, but neither model reproduced the observed planar magnetic structures. (4) The WSA-Enlil results of azimuthal magnetic field orientation are in better agreement with observations than those based on the MAS-Enlil. We suggest that the evolution of meridional tilt from ACE to Ulysses does not agree with projections because the parent coronal holes were highly structured. We also suggest that observations of azimuthal tilt do not agree with the model results because the models may underestimate transverse flows, whereas in reality, these flows could affect the observed azimuthal tilt of the CIR. The local orientation of PMSs within CIRs may also be distorted by transients, but their effect is unclear.
C1 [Broiles, T. W.; Desai, M. I.] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX USA.
[Broiles, T. W.; Desai, M. I.] SW Res Inst, Space Sci & Engn Div, 6220 Culebra Rd, San Antonio, TX 78238 USA.
[Lee, C. O.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02167 USA.
[Lee, C. O.] Air Force Res Lab, Space Vehicles Directorate, Albuquerque, NM USA.
[MacNeice, P. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Broiles, TW (reprint author), SW Res Inst, Space Sci & Engn Div, 6220 Culebra Rd, San Antonio, TX 78238 USA.
EM tbroiles@swri.edu
OI Broiles, Thomas/0000-0001-6910-2724; Lee, Christina/0000-0002-1604-3326
FU NASA [NNX08AK87G, NNX07AG85G]; NSF [NSF-ATM 0962666]
FX Work at the Southwest Research Institute has been supported by the NASA
grants NNX08AK87G and NNX07AG85G and the NSF grant NSF-ATM 0962666. We
thank the instrument teams and PIs for SWEPAM (D.J. McComas), SWOOPS
(D.J. McComas), MAG (C. W. Smith), and FGM (A. Balogh) for their work.
Additionally, we recognize M. A. Lee, the CCMC, D. Odstrcil, C.N. Arge,
Y.M. Wang, N.R. Sheeley, and R. Lionello, all of whom have made this
work possible.
NR 41
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Z9 4
U1 0
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 AUG
PY 2013
VL 118
IS 8
BP 4776
EP 4792
DI 10.1002/jgra.50482
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 225VK
UT WOS:000324992300007
ER
PT J
AU Walsh, BM
Sibeck, DG
Nishimura, Y
Angelopoulos, V
AF Walsh, B. M.
Sibeck, D. G.
Nishimura, Y.
Angelopoulos, V.
TI Statistical analysis of the plasmaspheric plume at the magnetopause
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE reconnection; plume; magnetopause
ID DAYSIDE MAGNETOPAUSE; MAGNETIC SHEAR; BOUNDARY-LAYER; IMAGE-RPI;
PLASMAPAUSE; INSTRUMENT; THEMIS; IONS; MAGNETOSPHERE; CONVECTION
AB During times of enhanced magnetospheric convection, cold dense plasma from the plasmasphere can form a plume extending sunward toward the dayside magnetopause. A statistical study is presented of cold high-density plasmaspheric plasma at the magnetopause. Observations from the Time History of Events and Macroscale Interactions (THEMIS) spacecraft show the plume to be present at the dayside magnetopause during 12.5% (148 of 1184) of the crossings. Its most common location in magnetic local time when contacting the magnetopause is at 13.6 h. The magnetopause crossings show evidence for reconnection in 68% of events with the plume while only 47% of events without plume. Although the plume is more likely to be observed at the magnetopause when reconnection is occurring, the typical reconnection jet velocity is lower for plume events than nonplume events, indicating the presence of the plume may be slowing the efficiency of the reconnection process.
C1 [Walsh, B. M.; Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nishimura, Y.; Angelopoulos, V.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
RP Walsh, BM (reprint author), NASA, Goddard Space Flight Ctr, Heliospher Div, Greenbelt, MD 20771 USA.
EM brian.walsh@nasa.gov
RI Walsh, Brian/C-4899-2016
OI Walsh, Brian/0000-0001-7426-5413
FU National Science Foundation [AGS-1136827]; NASA [NAS5-02099]
FX We thank J. Borovsky and M. Denton for the use of their geosynchronous
plume database. Support was given by the National Science Foundation
through grant AGS-1136827. We acknowledge NASA contract NAS5-02099 and
instrument teams for the use of the data from the THEMIS Mission,
Specifically, C. W. Carlson and J. P. McFadden for the use of ESA data,
J. W. Bonnell and F. S. Mozer for the use of EFI data, and K. H.
Glassmeier, U. Auster, and W. Baumjohann for the use of FGM data. We
also thank the Danish Meteorological Institute and the Arctic and
Antarctic Research Institute for providing the Polar Cap index.
NR 49
TC 23
Z9 23
U1 1
U2 8
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 AUG
PY 2013
VL 118
IS 8
BP 4844
EP 4851
DI 10.1002/jgra.50458
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 225VK
UT WOS:000324992300012
ER
PT J
AU Komar, CM
Cassak, PA
Dorelli, JC
Glocer, A
Kuznetsova, MM
AF Komar, C. M.
Cassak, P. A.
Dorelli, J. C.
Glocer, A.
Kuznetsova, M. M.
TI Tracing magnetic separators and their dependence on IMF clock angle in
global magnetospheric simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE magnetic separators; dayside magnetopause; magnetic reconnection
ID INTERPLANETARY FIELD; RECONNECTION; NULLS; LINE
AB A new, efficient, and highly accurate method for tracing magnetic separators in global magnetospheric simulations with arbitrary clock angle is presented. The technique is to begin at a magnetic null and iteratively march along the separator by finding where four magnetic topologies meet on a spherical surface. The technique is verified using exact solutions for separators resulting from an analytic magnetic field model that superposes dipolar and uniform magnetic fields. Global resistive magnetohydrodynamic simulations are performed using the three-dimensional Block-Adaptive Tree Solar-wind Roe-type Upwind Scheme code with a uniform resistivity, in eight distinct simulations with interplanetary magnetic field (IMF) clock angles ranging from 0 degrees (parallel) to 180 degrees (antiparallel). Magnetic nulls and separators are found in the simulations, and it is shown that separators traced here are accurate for any clock angle, unlike the last closed field line on the Sun-Earth line that fails for southward IMF. Trends in magnetic null locations and the structure of magnetic separators as a function of clock angle are presented and compared with those from the analytic field model. There are many qualitative similarities between the two models, but quantitative differences are also noted. Dependence on solar wind density is briefly investigated.
C1 [Komar, C. M.; Cassak, P. A.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
[Dorelli, J. C.; Glocer, A.; Kuznetsova, M. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Komar, CM (reprint author), W Virginia Univ, Dept Phys & Astron, White Hall,Box 6315, Morgantown, WV 26506 USA.
EM ckomar@mix.wvu.edu
RI Komar, Colin/K-5610-2013; Glocer, Alex/C-9512-2012; Dorelli,
John/C-9488-2012; feggans, john/F-5370-2012
OI Komar, Colin/0000-0001-5850-7507; Glocer, Alex/0000-0001-9843-9094;
FU NSF [AGS-0953463]; NASA [NNX10AN08A]; NASA West Virginia Space Grant
Consortium
FX Support from NSF grant AGS-0953463 (CMK and PAC), NASA grant NNX10AN08A
(PAC), and NASA West Virginia Space Grant Consortium (CMK) are
gratefully acknowledged. Simulations were performed at the Community
Coordinated Modeling Center at Goddard Space Flight Center through their
public Runs on Request system (http://ccmc.gsfc.nasa.gov). The CCMC is a
multiagency partnership between NASA, AFMC, AFOSR, AFRL, AFWA, NOAA,
NSF, and ONR. The BATS-R-US Model was developed by the Center for Space
Environment Modeling at the University of Michigan. A large portion of
the analysis presented here was made possible via the Kameleon and Space
Weather Explorer software packages provided by the CCMC. The Kameleon
software has been provided by the Community Coordinated Modeling Center
at NASA Goddard Space Flight Center (http://ccmc.gsfc.nasa.gov) Software
Developers: Marlo M. Maddox, David H. Berrios, and Lutz Rastaetter. The
authors would also like to thank M. Maddox and D. Berrios for their
software support and T. E. Moore for interesting discussions. Travel
support to the 2013 Geospace Environment Modeling (GEM) Summer Workshop
from NSF, CCMC, and GEM is gratefully acknowledged (CMK).
NR 40
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U1 0
U2 12
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 AUG
PY 2013
VL 118
IS 8
BP 4998
EP 5007
DI 10.1002/jgra.50479
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 225VK
UT WOS:000324992300025
ER
PT J
AU Benson, RF
Vinas, AF
Osherovich, VA
Fainberg, J
Purser, CM
Adrian, ML
Galkin, IA
Reinisch, BW
AF Benson, Robert F.
Vinas, Adolfo F.
Osherovich, Vladimir A.
Fainberg, Joseph
Purser, Carola M.
Adrian, Mark L.
Galkin, Ivan A.
Reinisch, Bodo W.
TI Magnetospheric electron-velocity-distribution function information from
wave observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE magnetosphere; velocity-distribution; plasmapause; radio sounding
ID PLASMA DISPERSION FUNCTION; MAGNETIC-FIELD; IMAGE MISSION; RESONANCES;
DENSITY; EMISSIONS; DIAGNOSTICS; FREQUENCIES; WHISTLER; SOUNDER
AB The electron-velocity-distribution function was determined to be highly non-Maxwellian and more appropriate to a kappa distribution, with approximate to 2.0, near magnetic midnight in the low-latitude magnetosphere just outside a stable plasmasphere during extremely quiet geomagnetic conditions. The kappa results were based on sounder-stimulated Qn plasma resonances using the Radio Plasma Imager (RPI) on the IMAGE satellite; the state of the plasmasphere was determined from IMAGE/EUV observations. The Qn resonances correspond to the maximum frequencies of Bernstein-mode waves that are observed between the harmonics of the electron cyclotron frequency in the frequency domain above the upper-hybrid frequency. Here we present the results of a parametric investigation that included suprathermal electrons in the electron-velocity-distribution function used in the plasma-wave dispersion equation to calculate the Qn frequencies for a range of kappa and f(pe)/f(ce) values for Qn resonances from Q1 to Q9. The Qn frequencies were also calculated using a Maxwellian distribution, and they were found to be greater than those calculated using a kappa distribution with the frequency differences increasing with increasing n for a fixed and with decreasing for a fixed n. The calculated f(Qn) values have been incorporated into the RPI BinBrowser software providing a powerful tool for rapidly obtaining information on the nature of the magnetospheric electron-velocity-distribution function and the electron number density N-e. This capability enabled accurate (within a few percent) in situ N-e determinations to be made along the outbound orbital track as IMAGE moved away from the plasmapause. The extremely quiet geomagnetic conditions allowed IMAGE/EUV-extracted counts to be compared with the RPI-determined orbital-track N-e profile. The comparisons revealed remarkably similar N-e structures.
C1 [Benson, Robert F.; Vinas, Adolfo F.; Fainberg, Joseph; Adrian, Mark L.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Osherovich, Vladimir A.] CUA Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Greenbelt, MD USA.
[Purser, Carola M.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div,GEST,UMBC, Greenbelt, MD 20771 USA.
[Galkin, Ivan A.; Reinisch, Bodo W.] Univ Massachusetts, Ctr Atmospher Res, Lowell, MA USA.
[Reinisch, Bodo W.] Lowell Digisonde Int, Lowell, MA USA.
RP Benson, RF (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Code 673, Greenbelt, MD 20771 USA.
EM Robert.F.Benson@nasa.gov
FU NASA Geospace Program
FX This work was supported by the NASA Geospace Program. The authors are
also thankful to the two reviewers for their helpful comments.
NR 49
TC 5
Z9 5
U1 0
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 AUG
PY 2013
VL 118
IS 8
BP 5039
EP 5049
DI 10.1002/jgra.50459
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 225VK
UT WOS:000324992300028
ER
PT J
AU Kissinger, J
Wilder, FD
McPherron, RL
Hsu, TS
Baker, JBH
Kepko, L
AF Kissinger, J.
Wilder, F. D.
McPherron, R. L.
Hsu, T. -S.
Baker, J. B. H.
Kepko, L.
TI Statistical occurrence and dynamics of the Harang discontinuity during
steady magnetospheric convection
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE steady magnetospheric convection; Harang discontinuity; SuperDARN;
spatial superposition; substorms; convection
ID INTERPLANETARY MAGNETIC-FIELD; SUPERPOSED EPOCH ANALYSIS; IONOSPHERIC
CONVECTION; CURRENTS; DIRECTIONS; SUPERDARN; EVOLUTION; PATTERNS; ONSET
AB The Harang discontinuity is a longitudinally extended ionospheric signature near midnight of flow reversal from westward to eastward with decreasing latitude. Its occurrence indicates enhanced convection in the magnetotail that requires an upward field-aligned current from the ionosphere due to diamagnetic ion drift. Previous reports using event studies have been conflicting as to the occurrence of the Harang discontinuity during a mode of enhanced magnetotail response called steady magnetospheric convection (SMC). With a comprehensive list of SMC events from 1997 through 2007, we utilize data from the Super Dual Auroral Radar Network and a novel spatial superposition technique to statistically examine the occurrence of the Harang discontinuity during SMC events. We find that the statistical signature of the Harang discontinuity begins before SMC starts and strengthens as the SMC events progress. We also detail the typical size and strength of the Harang discontinuity and find that it is more pronounced during interplanetary magnetic field +B-y conditions.
C1 [Kissinger, J.; Kepko, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kissinger, J.; McPherron, R. L.; Hsu, T. -S.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Wilder, F. D.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Wilder, F. D.; Baker, J. B. H.] Virginia Polytech Inst & State Univ, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24061 USA.
RP Kissinger, J (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 674,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM jenni.kissinger@nasa.gov
RI Kepko, Larry/D-7747-2012
OI Kepko, Larry/0000-0002-4911-8208
FU NSF [ATM-0720422, ATM-0946900]; NASA [NNX07AF60G, NNX10AF25G,
NAS5-02099]; THEMIS program; NASA; NSF Atmospheric and Geospace Sciences
Postdoctoral Research Fellowship
FX We would like to thank the World Data Center for Geomagnetism, Kyoto for
the use of AL and AU data, as well as K. Ogilvie and A. Szabo for
providing WIND solar wind magnetic field and plasma data. Kissinger,
McPherron, and Hsu were funded by NSF grant ATM-0720422, NASA grants
NNX07AF60G and NNX10AF25G, and the THEMIS program, supported by NASA
contract NAS5-02099. This research was also 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. Wilder was funded by the NSF Atmospheric and Geospace
Sciences Postdoctoral Research Fellowship. Baker was funded by NSF grant
ATM-0946900.
NR 24
TC 2
Z9 2
U1 0
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 AUG
PY 2013
VL 118
IS 8
BP 5127
EP 5135
DI 10.1002/jgra.50503
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 225VK
UT WOS:000324992300036
ER
PT J
AU Fang, XH
Lummerzheim, D
Jackman, CH
AF Fang, Xiaohua
Lummerzheim, Dirk
Jackman, Charles H.
TI Proton impact ionization and a fast calculation method
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE proton precipitation; ionization; secondary electrons; parameterization
ID H-ATOM FLUXES; TRANSPORT-THEORETIC MODEL; AURORAL PROTON;
UPPER-ATMOSPHERE; ION-PAIR; PRECIPITATION; HYDROGEN; ENERGY;
DEGRADATION; IONOSPHERE
AB We present a coupled Monte Carlo and multistream model simulating primary ionization and secondary electron ionization, respectively, from energetic proton precipitation in the Earth's upper atmosphere. Good agreement is obtained with previous model results. It is found that while secondary electrons make a negligible contribution to ionization from low-energy (10 keV) auroral proton precipitation, their importance increases with increasing incident proton energy, confirming earlier findings. It becomes significant or even comparable to primary ionization from protons and generated hydrogen atoms in charge-changing collisions. Our calculations of the mean energy loss per ion pair production show a nearly monotonic increase with incident proton energy, ranging from about 22 eV to 33 eV when incident energy increases from 100 eV to 1 MeV. To facilitate a fast calculation in large-scale computations, we develop a parameterization for total (primary plus secondary) ionization from monoenergetic proton precipitation. This is obtained by fitting to a large set of numerical results from the coupled model. The quick method applies to a wide energy range of 100 eV to 1 MeV for incident monoenergetic protons, and its validity has been extensively tested under a variety of background atmospheric conditions. Our new parameterization can be used to rapidly calculate the ionization altitude profile from precipitating protons with any spectral distributions without any significant compromise in accuracy. By considering branching ratios of ionized atmospheric species, the fast calculation method is thus useful for self-consistently including proton impact effects in large community models.
C1 [Fang, Xiaohua] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Lummerzheim, Dirk] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.
[Jackman, Charles H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Fang, XH (reprint author), Univ Colorado, Lab Atmospher & Space Phys, 3665 Discovey Dr, Boulder, CO 80303 USA.
EM xiaohua.fang@lasp.colorado.edu
RI Jackman, Charles/D-4699-2012; Fang, Xiaohua/C-2773-2008
OI Fang, Xiaohua/0000-0002-6584-2837
FU NASA [NNX09AI04G]
FX The work was supported by NASA grant NNX09AI04G.
NR 34
TC 4
Z9 4
U1 0
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 AUG
PY 2013
VL 118
IS 8
BP 5369
EP 5378
DI 10.1002/jgra.50484
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 225VK
UT WOS:000324992300059
ER
PT J
AU Guan, B
Molotch, NP
Waliser, DE
Jepsen, SM
Painter, TH
Dozier, J
AF Guan, Bin
Molotch, Noah P.
Waliser, Duane E.
Jepsen, Steven M.
Painter, Thomas H.
Dozier, Jeff
TI Snow water equivalent in the Sierra Nevada: Blending snow sensor
observations with snowmelt model simulations
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE snow water equivalent; snowmelt model; Sierra Nevada
ID RADIATIVE-TRANSFER CODE; DIGITAL ELEVATION DATA; RIO-GRANDE HEADWATERS;
COLORADO RIVER-BASIN; SPATIAL-DISTRIBUTION; COVER DATA; ATMOSPHERIC
CORRECTION; HYDROLOGIC IMPACTS; VECTOR VERSION; SATELLITE DATA
AB We estimate the spatial distribution of daily melt-season snow water equivalent (SWE) over the Sierra Nevada for March to August, 2000-2012, by two methods: reconstruction by combining remotely sensed snow cover images with a spatially distributed snowmelt model and a blended method in which the reconstruction is combined with in situ snow sensor observations. We validate the methods with 17 snow surveys at six locations with spatial sampling and with the operational snow sensor network. We also compare the methods with NOAA's operational Snow Data Assimilation System (SNODAS). Mean biases of the methods compared to the snow surveys are -0.193 m (reconstruction), 0.001 m (blended), and -0.181 m (SNODAS). Corresponding root-mean-square errors are 0.252, 0.205, and 0.254 m. Comparison between blended and snow sensor SWE suggests that the current sensor network inadequately represents SWE in the Sierra Nevada because of the low spatial density of sensors in the lower/higher elevations. Mean correlation with streamflow in 19 Sierra Nevada watersheds is better with reconstructed SWE (r=0.91) versus blended SWE (r=0.81), snow sensor SWE (r=0.85), and SNODAS SWE (r=0.86). On the other hand, the correlation with blended SWE is generally better than with reconstructed, snow sensor, and SNODAS SWE late in the snowmelt season when snow sensors report zero SWE but snow remains in the higher elevations. Sensitivity tests indicate downwelling longwave radiation, snow albedo, forest density, and turbulent fluxes are potentially important sources of errors/uncertainties in reconstructed SWE, and domain-mean blended SWE is relatively insensitive to the number of snow sensors blended.
Key Points
The blended SWE product is more accurate than the NOAA SWE product Satellite-based snow cover depletion data improves SWE estimation Sensitivity tests suggest four key sources of uncertainties in reconstructed SWE
C1 [Guan, Bin; Molotch, Noah P.; Waliser, Duane E.; Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Guan, Bin] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Jepsen, Steven M.] Univ Calif, Sierra Nevada Res Inst, Merced, CA USA.
[Dozier, Jeff] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA.
RP Guan, B (reprint author), CALTECH, Jet Prop Lab, M-S 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM bin.guan@jpl.nasa.gov
RI Guan, Bin/F-6735-2010; Painter, Thomas/B-7806-2016; Molotch,
Noah/C-8576-2009; Dozier, Jeff/B-7364-2009
OI Dozier, Jeff/0000-0001-8542-431X
FU NASA [NNX08AH18G, NNX11AK35A, NNX11AK35G, NNX10AO97G]; NSF [EAR 1032295,
EAR 1141764]; USDA [2012-67003-19802]; NOAA RISA Western Water
Assessment; United States American Recovery and Reinvestment Act funds
FX This research was supported by NASA grants NNX08AH18G, NNX11AK35A,
NNX11AK35G, and NNX10AO97G, NSF grants EAR 1032295 and EAR 1141764, USDA
grant 2012-67003-19802, the NOAA RISA Western Water Assessment, and
United States American Recovery and Reinvestment Act funds. Gridded snow
survey data from five sites are provided by L. Meromy, S. Roberts, and
J. Sickman. L. Lestak provided technical support. D.E.W.'s and B.G.'s
contributions, and part of N.P.M.'s, S.M.J.'s and T.H.P.'s
contributions, to this study were carried out on behalf of the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 72
TC 25
Z9 25
U1 4
U2 45
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
J9 WATER RESOUR RES
JI Water Resour. Res.
PD AUG
PY 2013
VL 49
IS 8
BP 5029
EP 5046
DI 10.1002/wrcr.20387
PG 18
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 223VA
UT WOS:000324838300038
ER
PT J
AU O'Loughlin, F
Trigg, MA
Schumann, GJP
Bates, PD
AF O'Loughlin, F.
Trigg, M. A.
Schumann, G. J. -P.
Bates, P. D.
TI Hydraulic characterization of the middle reach of the Congo River
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE Congo River; river characteristics; water surface slopes; backwater
effects; river hydraulics
ID SATELLITE RADAR ALTIMETRY; CENTRAL-AFRICA; WATER DYNAMICS; AMAZON RIVER;
ZAIRE BASIN; IMAGERY; HISTORY; CHANNEL; SYSTEM; BRAZIL
AB The middle reach of the Congo remains one of the most difficult places to access, with ongoing conflicts and a lack of infrastructure. This has resulted in the Congo being perhaps the least understood large river hydraulically, particularly compared to the Amazon, Nile, or Mississippi. Globally the Congo River is important; it is the largest river in Africa and the basin contains some of the largest areas of tropical forests and wetlands in the world, which are important to both the global carbon and methane cycles. This study produced the first detailed hydraulic characterization of the middle reach, utilizing mostly remotely sensed data sets. Using Landsat imagery, a 30 m resolution water-mask was created for the middle reach, from which effective river widths and the number of channels and islands were determined. Water surface slopes were determined using ICESat observations for three different periods during the annual flood pulse, and while the overall slope calculated was similar to previous estimates, greater spatial variability was identified. We find that the water surface slope varies markedly in space but relatively little in time and that this appears to contrast with the Amazon where previous studies indicate that time and spatial variations are of equal magnitude. Five key hydraulic constraints were also identified, which play an important role in the overall dynamics of the Congo. Finally, backwater lengths were approximated for four of these constraints, with the results showing that at high water, over a third of the middle reach is affected by backwater effects.
Key Points
Previous methods of river widths fail to account for the spatial variability Water surface slopes of the Congo are more varied spatially than temporally Backwater affects over a third of the middle reach of the Congo at high water
C1 [O'Loughlin, F.; Trigg, M. A.; Bates, P. D.] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
[Schumann, G. J. -P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP O'Loughlin, F (reprint author), Univ Bristol, Sch Geog Sci, Univ Rd, Bristol BS8 1SS, Avon, England.
EM fiachra.oloughlin@bristol.ac.uk
RI Bates, Paul/C-8026-2012; O'Loughlin, Fiachra/G-8858-2013; Schumann,
Guy/F-9760-2011; Trigg, Mark/A-5898-2010
OI Bates, Paul/0000-0001-9192-9963; O'Loughlin,
Fiachra/0000-0002-9435-8278; Trigg, Mark/0000-0002-8412-9332
FU Leverhulme Trust; Willis Research Network
FX The work in this paper was supported by a research grant from the
Leverhulme Trust. The work by G. Schumann 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 Ir. Georges Gulemvuga, Director of Water
Resources for the International Commission for the Congo-Ubangui-Sangha
Basin, for providing the stage level data used in this study. Mark Trigg
is funded by the Willis Research Network. Finally, the authors would
like to thank Doug Alsdorf and other anonymous reviewers for their
constructive comments.
NR 34
TC 19
Z9 19
U1 1
U2 21
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 AUG
PY 2013
VL 49
IS 8
BP 5059
EP 5070
DI 10.1002/wrcr.20398
PG 12
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 223VA
UT WOS:000324838300040
ER
PT J
AU Fu, YN
Freymueller, JT
AF Fu, Yuning
Freymueller, Jeffrey T.
TI Repeated large Slow Slip Events at the southcentral Alaska subduction
zone
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Slow Slip Event; Alaska subduction zone; GPS; transient deformation
ID SILENT SLIP; DEFORMATION; JAPAN; EARTHQUAKES; PENINSULA; INTERFACE;
BENEATH; SPACE
AB We identify and study an ongoing Slow Slip Event (SSE) in the southcentral Alaska subduction zone using GPS measurements. This is the second large SSE in this region since modern geodetic measurements became available in 1993. We divide the ongoing SSE into two phases according to their transient displacement time evolution; their slip distributions are similar to each other but slip rates are slightly different. This ongoing SSE occurs downdip of the main asperity that ruptured in the 1964 Alaska earthquake, on the same part of the subduction interface as the earlier 1998-2001 SSE. The average slip rate of this SSE is similar to 4-5 cm/yr, with a cumulative moment magnitude of Mw 7.5 (Mw 7.3 and Mw 7.1 For Phases I and II, respectively) through the end of 2012. The time and space dependence of the GPS displacements suggest that the slip area remained nearly the same during Phase I, while the slip rate increased with time. The SSEs occur on a transitional section of the subduction plate interface between the fully locked updip part and the freely slipping deeper part. During the 1964 earthquake, slip on the region of the SSE was much lower than slip in the updip region. Based on this observation and the repeated SSEs, we conclude that this part of the interface slips repeatedly in SSEs throughout the interseismic period and does not build up a large slip deficit to be released through large slip in earthquakes. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Fu, Yuning; Freymueller, Jeffrey T.] Univ Alaska, Inst Geophys, Fairbanks, AK 99701 USA.
RP Fu, YN (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM yuning@gi.alaska.edu
FU NSF [EAR-1215933]; Global Change Student Grant
FX The authors are grateful to Donald Argus for helpful discussions and
suggestions. We thank the Slab1.0 team for sharing their subduction slab
geometry data. We appreciate two anonymous reviews for comments that
significantly improve the manuscripts. This work was supported by NSF
Grant EAR-1215933 to JTF, and a Global Change Student Grant to YF.
NR 27
TC 18
Z9 19
U1 1
U2 15
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD AUG 1
PY 2013
VL 375
BP 303
EP 311
DI 10.1016/j.epsl.2013.05.049
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 223YB
UT WOS:000324847300027
ER
PT J
AU Hall, HJ
AF Hall, Helen J.
TI Ground-Based/Airborne Telescopes and Instrumentation
SO OPTICAL ENGINEERING
LA English
DT Editorial Material
C1 NASA, Ames Res Ctr, SOFIA, USRA, Moffett Field, CA 94035 USA.
RP Hall, HJ (reprint author), NASA, Ames Res Ctr, SOFIA, USRA, Bldg N232,MS 232-12, Moffett Field, CA 94035 USA.
EM hhall@sofia.usra.edu
NR 0
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 0091-3286
J9 OPT ENG
JI Opt. Eng.
PD AUG
PY 2013
VL 52
IS 8
AR 081601
DI 10.1117/1.OE.52.8.081601
PG 1
WC Optics
SC Optics
GA 216NP
UT WOS:000324290900005
ER
PT J
AU Akyuz, A
Thompson, DJ
Donato, D
Perkins, JS
Fuhrmann, L
Angelakis, E
Zensus, JA
Larsson, S
Sokolovsky, K
Kurtanidze, O
AF Akyuz, A.
Thompson, D. J.
Donato, D.
Perkins, J. S.
Fuhrmann, L.
Angelakis, E.
Zensus, J. A.
Larsson, S.
Sokolovsky, K.
Kurtanidze, O.
TI Long-term multiwavelength studies of high-redshift blazar 0836+710
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; gamma rays: galaxies; quasars: individual: 0836+710
ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; FERMI-DETECTED BLAZARS;
GAMMA-RAY OUTBURSTS; X-RAY; COMPLETE SAMPLE; SOURCE CATALOG; 3C 279;
RADIO; SWIFT
AB Aims. The observation of gamma-ray flares from blazar 0836+710 in 2011, following a period of quiescence, offered an opportunity to study correlated activity at different wavelengths for a high-redshift (z = 2.218) active galactic nucleus.
Methods. Optical and radio monitoring, plus Fermi-LAT gamma-ray monitoring provided 2008-2012 coverage, while Swift offered auxiliary optical, ultraviolet, and X-ray information. Other contemporaneous observations were used to construct a broad-band spectral energy distribution.
Results. There is evidence of correlation but not a measurable lag between the optical and.-ray flaring emission. In contrast, there is no clear correlation between radio and gamma-ray activity, indicating radio emission regions that are unrelated to the parts of the jet that produce the gamma rays. The gamma-ray energy spectrum is unusual in showing a change of shape from a power law to a curved spectrum when going from the quiescent state to the active state.
C1 [Akyuz, A.] Cukurova Univ, Dept Phys, TR-01330 Adana, Turkey.
[Akyuz, A.; Thompson, D. J.; Donato, D.; Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Donato, D.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA.
[Perkins, J. S.] Univ Maryland Baltimore Cty, CSST, CRESST, Baltimore, MD 21250 USA.
[Fuhrmann, L.; Angelakis, E.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Larsson, S.] Stockholm Univ, AlbaNova, Dept Phys, S-10691 Stockholm, Sweden.
[Larsson, S.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, S-10691 Stockholm, Sweden.
[Larsson, S.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden.
[Sokolovsky, K.] Astro Space Ctr Lebedev Phys Inst, Moscow 117997, Russia.
[Sokolovsky, K.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Kurtanidze, O.] Abastumani Observ, GE-383762 Abastumani, Rep of Georgia.
[Kurtanidze, O.] Heidelberg Univ, Zentrum Astron, D-69117 Heidelberg, Germany.
[Kurtanidze, O.] Kazan Fed Univ, Engelhardt Astron Observ, Tatarstan, Russia.
RP Akyuz, A (reprint author), Cukurova Univ, Dept Phys, TR-01330 Adana, Turkey.
EM aakyuz@cu.edu.tr; David.J.Thompson@nasa.gov
RI Kurtanidze, Omar/J-6237-2014; Sokolovsky, Kirill/D-2246-2015
OI Sokolovsky, Kirill/0000-0001-5991-6863
FU German Deutsche Forschungsgemeinschaft, DFG [Ts 17/2-1]; National
Aeronautics and Space Administration; Georgian National Science
Foundation [GNSF/ST09/5214-320]; COST Action [MP0905]; Council of Higher
Education in Turkey
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 is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France. This
research is partly based on observations with the 100-m telescope of the
MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg. This work
has made use of observations with the IRAM 30-m telescope. Part of this
work was supported by the German Deutsche Forschungsgemeinschaft, DFG
project number Ts 17/2-1. This work made use of data supplied by the UK
Swift Science Data Centre at the University of Leicester. 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. The Abastumani Observatory team acknowledges financial
support by the Georgian National Science Foundation through grant
GNSF/ST09/5214-320. Part of this work was supported by the COST Action
MP0905, "Black Holes in a Violent Universe". A. Akyuz acknowledges
financial support by The Council of Higher Education in Turkey. The
authors extend special thanks to F. D'Ammando for many helpful
suggestions during the preparation of this manuscript.
NR 53
TC 1
Z9 1
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 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2013
VL 556
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211GH
UT WOS:000323893500071
ER
PT J
AU Aleksic, J
Antonelli, LA
Antoranz, P
Asensio, M
Backes, M
de Almeida, UB
Barrio, JA
Bednarek, W
Berger, K
Bernardini, E
Biland, A
Blanch, O
Bock, RK
Boller, A
Bonnefoy, S
Bonnoli, G
Tridon, DB
Bretz, T
Carmona, E
Carosi, A
Fidalgo, DC
Colin, P
Colombo, E
Contreras, JL
Cortina, J
Cossio, L
Covino, S
Da Vela, P
Dazzi, F
De Angelis, A
De Caneva, G
De Lotto, B
Mendez, CD
Doert, M
Dominguez, A
Prester, DD
Dorner, D
Doro, M
Eisenacher, D
Elsaesser, D
Ferenc, D
Fonseca, MV
Font, L
Fruck, C
Lopez, RJG
Garczarczyk, M
Terrats, DG
Gaug, M
Giavitto, G
Godinovic, N
Munoz, AG
Gozzini, SR
Hadamek, A
Hadasch, D
Herrero, A
Hose, J
Hrupec, D
Jankowski, F
Kadenius, V
Klepser, S
Knoetig, ML
Kraehenbuehl, T
Krause, J
Kushida, J
La Barbera, A
Lelas, D
Leonardo, E
Lewandowska, N
Lindfors, E
Lombardi, S
Lopez, M
Lopez-Coto, R
Lopez-Oramas, A
Lorenz, E
Lozano, I
Makariev, M
Mallot, K
Maneva, G
Mankuzhiyil, N
Mannheim, K
Maraschi, L
Marcote, B
Mariotti, M
Martinez, M
Masbou, J
Mazin, D
Meucci, M
Miranda, JM
Mirzoyan, R
Moldon, J
Moralejo, A
Munar-Adrover, P
Nakajima, D
Niedzwiecki, A
Nieto, D
Nilsson, K
Nowak, N
Orito, R
Paiano, S
Palatiello, M
Paneque, D
Paoletti, R
Paredes, JM
Partini, S
Persic, M
Pilia, M
Prada, F
PradaMoroni, PG
Prandini, E
Puljak, I
Reichardt, I
Reinthal, R
Rhode, W
Ribo, M
Rico, J
Rugamer, S
Saggion, A
Saito, K
Saito, TY
Salvati, M
Satalecka, K
Scalzotto, V
Scapin, V
Schultz, C
Schweizer, T
Shore, SN
Sillanpaa, A
Sitarek, J
Snidaric, I
Sobczynska, D
Spanier, F
Spiro, S
Stamatescu, V
Stamerra, A
Steinke, B
Storz, J
Sun, S
Suric, T
Takalo, L
Takami, H
Tavecchio, F
Temnikov, P
Terzic, T
Tescaro, D
Teshima, M
Tibolla, O
Torres, DF
Toyama, T
Treves, A
Uellenbeck, M
Vogler, P
Wagner, RM
Weitzel, Q
Zandanel, F
Zanin, R
Longo, F
Lucarelli, F
Pittori, C
Vercellone, S
Bastieri, D
Sbarra, C
Angelakis, E
Fuhrmann, L
Nestoras, I
Krichbaum, TP
Sievers, A
Zensus, JA
Antonyuk, KA
Baumgartner, W
Berduygin, A
Carini, M
Cook, K
Gehrels, N
Kadler, M
Kovalev, YA
Kovalev, YY
Krauss, F
Krimm, HA
Lahteenmaki, A
Lister, ML
Max-Moerbeck, W
Pasanen, M
Pushkarev, AB
Readhead, ACS
Richards, JL
Sainio, J
Shakhovskoy, DN
Sokolovsky, KV
Tornikoski, M
Tueller, J
Weidinger, M
Wilms, J
AF Aleksic, J.
Antonelli, L. A.
Antoranz, P.
Asensio, M.
Backes, M.
de Almeida, U. Barres
Barrio, J. A.
Bednarek, W.
Berger, K.
Bernardini, E.
Biland, A.
Blanch, O.
Bock, R. K.
Boller, A.
Bonnefoy, S.
Bonnoli, G.
Tridon, D. Borla
Bretz, T.
Carmona, E.
Carosi, A.
Fidalgo, D. Carreto
Colin, P.
Colombo, E.
Contreras, J. L.
Cortina, J.
Cossio, L.
Covino, S.
Da Vela, P.
Dazzi, F.
De Angelis, A.
De Caneva, G.
De Lotto, B.
Mendez, C. Delgado
Doert, M.
Dominguez, A.
Prester, D. Dominis
Dorner, D.
Doro, M.
Eisenacher, D.
Elsaesser, D.
Ferenc, D.
Fonseca, M. V.
Font, L.
Fruck, C.
Lopez, R. J. Garcia
Garczarczyk, M.
Terrats, D. Garrido
Gaug, M.
Giavitto, G.
Godinovic, N.
Munoz, A. Gonzalez
Gozzini, S. R.
Hadamek, A.
Hadasch, D.
Herrero, A.
Hose, J.
Hrupec, D.
Jankowski, F.
Kadenius, V.
Klepser, S.
Knoetig, M. L.
Kraehenbuehl, T.
Krause, J.
Kushida, J.
La Barbera, A.
Lelas, D.
Leonardo, E.
Lewandowska, N.
Lindfors, E.
Lombardi, S.
Lopez, M.
Lopez-Coto, R.
Lopez-Oramas, A.
Lorenz, E.
Lozano, I.
Makariev, M.
Mallot, K.
Maneva, G.
Mankuzhiyil, N.
Mannheim, K.
Maraschi, L.
Marcote, B.
Mariotti, M.
Martinez, M.
Masbou, J.
Mazin, D.
Meucci, M.
Miranda, J. M.
Mirzoyan, R.
Moldon, J.
Moralejo, A.
Munar-Adrover, P.
Nakajima, D.
Niedzwiecki, A.
Nieto, D.
Nilsson, K.
Nowak, N.
Orito, R.
Paiano, S.
Palatiello, M.
Paneque, D.
Paoletti, R.
Paredes, J. M.
Partini, S.
Persic, M.
Pilia, M.
Prada, F.
PradaMoroni, P. G.
Prandini, E.
Puljak, I.
Reichardt, I.
Reinthal, R.
Rhode, W.
Ribo, M.
Rico, J.
Ruegamer, S.
Saggion, A.
Saito, K.
Saito, T. Y.
Salvati, M.
Satalecka, K.
Scalzotto, V.
Scapin, V.
Schultz, C.
Schweizer, T.
Shore, S. N.
Sillanpaa, A.
Sitarek, J.
Snidaric, I.
Sobczynska, D.
Spanier, F.
Spiro, S.
Stamatescu, V.
Stamerra, A.
Steinke, B.
Storz, J.
Sun, S.
Suric, T.
Takalo, L.
Takami, H.
Tavecchio, F.
Temnikov, P.
Terzic, T.
Tescaro, D.
Teshima, M.
Tibolla, O.
Torres, D. F.
Toyama, T.
Treves, A.
Uellenbeck, M.
Vogler, P.
Wagner, R. M.
Weitzel, Q.
Zandanel, F.
Zanin, R.
Longo, F.
Lucarelli, F.
Pittori, C.
Vercellone, S.
Bastieri, D.
Sbarra, C.
Angelakis, E.
Fuhrmann, L.
Nestoras, I.
Krichbaum, T. P.
Sievers, A.
Zensus, J. A.
Antonyuk, K. A.
Baumgartner, W.
Berduygin, A.
Carini, M.
Cook, K.
Gehrels, N.
Kadler, M.
Kovalev, Yu. A.
Kovalev, Y. Y.
Krauss, F.
Krimm, H. A.
Lahteenmaki, A.
Lister, M. L.
Max-Moerbeck, W.
Pasanen, M.
Pushkarev, A. B.
Readhead, A. C. S.
Richards, J. L.
Sainio, J.
Shakhovskoy, D. N.
Sokolovsky, K. V.
Tornikoski, M.
Tueller, J.
Weidinger, M.
Wilms, J.
CA MAGIC Collaboration
AGILE Team
Fermi-LAT Collaboration
F-GAMMA Program
TI The simultaneous low state spectral energy distribution of 1ES 2344+514
from radio to very high energies
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; BL Lacertae objects: individual: 1ES 2344+514; gamma
rays: galaxies; X-rays: individuals: 1ES 2344+514; radiation mechanisms:
non-thermal
ID ACTIVE GALACTIC NUCLEI; BL-LACERTAE OBJECTS; GAMMA-RAY EMISSION;
LARGE-AREA TELESCOPE; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS;
SELF-COMPTON MODEL; X-RAY; LAC OBJECTS; RELATIVISTIC JETS; MARKARIAN 501
AB Context. BL Lacertae objects are variable at all energy bands on time scales down to minutes. To construct and interpret their spectral energy distribution (SED), simultaneous broad-band observations are mandatory. Up to now, the number of objects studied during such campaigns is very limited and biased towards high flux states.
Aims. We present the results of a dedicated multi-wavelength study of the high-frequency peaked BL Lacertae (HBL) object and known TeV emitter 1ES 2344+514 by means of a pre-organised campaign.
Methods. The observations were conducted during simultaneous visibility windows of MAGIC and AGILE in late 2008. The measurements were complemented by Mets hovi, RATAN-600, KVA+Tuorla, Swift and VLBA pointings. Additional coverage was provided by the ongoing long-term F-GAMMA and MOJAVE programs, the OVRO 40-m and CrAO telescopes as well as the Fermi satellite. The obtained SEDs are modelled using a one-zone as well as a self-consistent two-zone synchrotron self-Compton model.
Results. 1ES 2344+514 was found at very low flux states in both X-rays and very high energy gamma rays. Variability was detected in the low frequency radio and X-ray bands only, where for the latter a small flare was observed. The X-ray flare was possibly caused by shock acceleration characterised by similar cooling and acceleration time scales. MOJAVE VLBA monitoring reveals a static jet whose components are stable over time scales of eleven years, contrary to previous findings. There appears to be no significant correlation between the 15 GHz and R-band monitoring light curves. The observations presented here constitute the first multi-wavelength campaign on 1ES 2344+514 from radio to VHE energies and one of the few simultaneous SEDs during low activity states. The quasi-simultaneous Fermi-LAT data poses some challenges for SED modelling, but in general the SEDs are described well by both applied models. The resulting parameters are typical for TeV emitting HBLs. Consequently it remains unclear whether a so-called quiescent state was found in this campaign.
C1 [Aleksic, J.; Blanch, O.; Cortina, J.; Giavitto, G.; Munoz, A. Gonzalez; Klepser, S.; Lopez-Coto, R.; Lopez-Oramas, A.; Martinez, M.; Moralejo, A.; Reichardt, I.; Rico, J.; Sitarek, J.; Stamatescu, V.] IFAE, Bellaterra 08193, Spain.
[Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; La Barbera, A.; Lombardi, S.; Maraschi, L.; Salvati, M.; Spiro, S.; Tavecchio, F.] INAF Natl Inst Astrophys, I-00136 Rome, Italy.
[Antoranz, P.; Da Vela, P.; Leonardo, E.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Stamerra, A.] Univ Siena, I-53100 Siena, Italy.
[Antoranz, P.; Da Vela, P.; Leonardo, E.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Stamerra, A.] INFN Pisa, I-53100 Siena, Italy.
[Asensio, M.; Barrio, J. A.; Bonnefoy, S.; Fidalgo, D. Carreto; Contreras, J. L.; Fonseca, M. V.; Lopez, M.; Lozano, I.; Nieto, D.; Satalecka, K.; Scapin, V.] Univ Complutense, E-28040 Madrid, Spain.
[Backes, M.; Doert, M.; Hadamek, A.; Rhode, W.; Uellenbeck, M.] Tech Univ Dortmund, D-44221 Dortmund, Germany.
[Tridon, D. Borla; Colin, P.; Fruck, C.; Hose, J.; Knoetig, M. L.; Krause, J.; Lorenz, E.; Mazin, D.; Mirzoyan, R.; Nakajima, D.; Nowak, N.; Paneque, D.; Steinke, B.; Teshima, M.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Bednarek, W.; Niedzwiecki, A.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Berger, K.; Colombo, E.; Lopez, R. J. Garcia; Garczarczyk, M.; Herrero, A.; Tescaro, D.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Berger, K.; Lopez, R. J. Garcia; Herrero, A.] Univ Laguna, Depto Astrofis, San Cristobal la Laguna, Spain.
[Bernardini, E.; De Caneva, G.; Gozzini, S. R.; Jankowski, F.; Mallot, K.] Deutsch Elekt Synchrotron DESY, D-15738 Zeuthen, Germany.
[Biland, A.; Boller, A.; Kraehenbuehl, T.; Lorenz, E.; Vogler, P.; Weitzel, Q.] ETH, CH-8093 Zurich, Switzerland.
[Bretz, T.; Fidalgo, D. Carreto; Dorner, D.; Eisenacher, D.; Elsaesser, D.; Lewandowska, N.; Mannheim, K.; Ruegamer, S.; Spanier, F.; Storz, J.; Tibolla, O.; Kadler, M.] Univ Wurzburg, D-97074 Wurzburg, Germany.
[Carmona, E.; Mendez, C. Delgado] Ctr Invest Energet Medioambient & Tecnol, Madrid 28040, Spain.
[Cossio, L.; Dazzi, F.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] Univ Udine, I-33100 Udine, Italy.
[Cossio, L.; Dazzi, F.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] INFN Trieste, I-33100 Udine, Italy.
[Dominguez, A.; Prada, F.; Zandanel, F.] Inst Astrofis Andalucia CSIC, Granada 18080, Spain.
[Prester, D. Dominis; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Suric, T.; Terzic, T.] Univ Rijeka, Croatian MAGIC Consortium, Rudjer Boskov Inst, Zagreb 10000, Croatia.
[Prester, D. Dominis; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Suric, T.; Terzic, T.] Univ Split, Zagreb 10000, Croatia.
[Doro, M.; Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, Bellaterra 08193, Spain.
[Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Bellaterra 08193, Spain.
[Kadenius, V.; Lindfors, E.; Nilsson, K.; Reinthal, R.; Sillanpaa, A.; Takalo, L.; Berduygin, A.; Pasanen, M.; Sainio, J.] Univ Turku, Tuorla Observ, Piikkio 21500, Finland.
[Kushida, J.; Orito, R.; Saito, K.; Takami, H.] Kyoto Univ, Div Phys & Astron, Japanese MAGIC Consortium, Kyoto, Japan.
[Makariev, M.; Maneva, G.; Temnikov, P.] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BU-1784 Sofia, Bulgaria.
[Marcote, B.; Moldon, J.; Munar-Adrover, P.; Paredes, J. M.; Ribo, M.; Zanin, R.] Univ Barcelona, ICC IEEC, E-08028 Barcelona, Spain.
[Mariotti, M.; Masbou, J.; Paiano, S.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.; Bastieri, D.] Univ Padua, I-35131 Padua, Italy.
[Mariotti, M.; Masbou, J.; Paiano, S.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.; Bastieri, D.] Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[Persic, M.] INAF Osservatorio Astron, I-34143 Trieste, Italy.
[Persic, M.] Ist Nazl Fis Nucl, I-34143 Trieste, Italy.
[Pilia, M.; Treves, A.] Univ Insubria, I-22100 Como, Italy.
[PradaMoroni, P. G.; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy.
[PradaMoroni, P. G.; Shore, S. N.] Ist Nazl Fis Nucl, Pisa, Italy.
[Rico, J.; Torres, D. F.] ICREA, Barcelona 08010, Spain.
[Bretz, T.] Ecole Polytech Fed Lausanne, CH-1015 Lausanne, Switzerland.
[Dazzi, F.] INFN Padova, Padua, Italy.
[Prada, F.] UAM, CSIC, Inst Fis Teor, Madrid 28049, Spain.
[Longo, F.] Univ Trieste, I-34127 Trieste, Italy.
[Longo, F.] Ist Nazl Fis Nucl, I-34127 Trieste, Italy.
[Lucarelli, F.; Pittori, C.] ASI, Sci Data Ctr, I-00040 Monte Porzio Catone, Italy.
[Lucarelli, F.; Pittori, C.] INAF Oar, I-00040 Monte Porzio Catone, Italy.
[Vercellone, S.] INAF, Ist Astrofis Spaziale Fis Cosm, I-90146 Palermo, Italy.
[Sbarra, C.] Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[Angelakis, E.; Fuhrmann, L.; Nestoras, I.; Krichbaum, T. P.; Zensus, J. A.; Kovalev, Y. Y.; Sokolovsky, K. V.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Sievers, A.] Inst Radio Astron Millimetr, Granada 18012, Spain.
[Antonyuk, K. A.; Pushkarev, A. B.; Shakhovskoy, D. N.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Ukraine.
[Baumgartner, W.; Gehrels, N.; Krimm, H. A.; Tueller, J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Carini, M.; Cook, K.] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA.
[Kovalev, Yu. A.; Kovalev, Y. Y.; Sokolovsky, K. V.] Astro Space Ctr Lebedev Phys Inst, Moscow 117997, Russia.
[Krauss, F.; Wilms, J.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany.
[Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Lahteenmaki, A.; Tornikoski, M.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland.
[Lister, M. L.; Richards, J. L.] Purdue Univ, Dept Phys, W Lafayette, IN USA.
[Max-Moerbeck, W.; Readhead, A. C. S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Pushkarev, A. B.] Pulkovo Observ, St Petersburg 196140, Russia.
[Sokolovsky, K. V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Weidinger, M.] Ruhr Univ Bochum, D-44780 Bochum, Germany.
RP Rugamer, S (reprint author), Univ Wurzburg, D-97074 Wurzburg, Germany.
EM elilin@utu.fi; snruegam@astro.uni-wuerzburg.de
RI Barrio, Juan/L-3227-2014; Martinez Rodriguez, Manel/C-2539-2017;
Cortina, Juan/C-2783-2017; Fonseca Gonzalez, Maria Victoria/I-2004-2015;
Delgado, Carlos/K-7587-2014; Kovalev, Yuri/N-1053-2015; Pushkarev,
Alexander/M-9997-2015; Pittori, Carlotta/C-7710-2016; Stamatescu,
Victor/C-9945-2016; Contreras Gonzalez, Jose Luis/K-7255-2014; Temnikov,
Petar/L-6999-2016; Maneva, Galina/L-7120-2016; Makariev,
Martin/M-2122-2016; Backes, Michael/N-5126-2016; Torres,
Diego/O-9422-2016; Reichardt, Ignasi/P-7478-2016; Munoz,
Alfonso/K-7823-2013; Kovalev, Yuri/J-5671-2013; Wilms,
Joern/C-8116-2013; Lahteenmaki, Anne/L-5987-2013; Rico,
Javier/K-8004-2014; Fernandez, Ester/K-9734-2014; Lopez Moya,
Marcos/L-2304-2014; Antoranz, Pedro/H-5095-2015; Miranda, Jose
Miguel/F-2913-2013; GAug, Markus/L-2340-2014; Font, Lluis/L-4197-2014;
Moralejo Olaizola, Abelardo/M-2916-2014; Ribo, Marc/B-3579-2015;
Sokolovsky, Kirill/D-2246-2015
OI Doro, Michele/0000-0001-9104-3214; Stamerra,
Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053;
Covino, Stefano/0000-0001-9078-5507; Paredes, Josep
M./0000-0002-1566-9044; Lucarelli, Fabrizio/0000-0002-6311-764X;
Jankowski, Fabian/0000-0002-6658-2811; Tavecchio,
Fabrizio/0000-0003-0256-0995; Bonnoli, Giacomo/0000-0003-2464-9077;
Nieto, Daniel/0000-0003-3343-0755; De Lotto,
Barbara/0000-0003-3624-4480; Spanier, Felix/0000-0001-6802-4744;
Bastieri, Denis/0000-0002-6954-8862; Ribo, Marc/0000-0002-9931-4557;
Ahnen, Max Ludwig/0000-0003-1000-0082; Angelakis,
Emmanouil/0000-0001-7327-5441; Kadler, Matthias/0000-0001-5606-6154;
Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452;
Dominguez, Alberto/0000-0002-3433-4610; Fonseca Gonzalez, Maria
Victoria/0000-0003-2235-0725; Prada Moroni, Pier
Giorgio/0000-0001-9712-9916; LA BARBERA, ANTONINO/0000-0002-5880-8913;
leonardo, elvira/0000-0003-0271-7673; Vercellone,
Stefano/0000-0003-1163-1396; Delgado, Carlos/0000-0002-7014-4101;
Pittori, Carlotta/0000-0001-6661-9779; Stamatescu,
Victor/0000-0001-9030-7513; Contreras Gonzalez, Jose
Luis/0000-0001-7282-2394; Temnikov, Petar/0000-0002-9559-3384; Backes,
Michael/0000-0002-9326-6400; Torres, Diego/0000-0002-1522-9065;
Reichardt, Ignasi/0000-0003-3694-3820; Munoz,
Alfonso/0000-0003-3347-6518; Kovalev, Yuri/0000-0001-9303-3263; Wilms,
Joern/0000-0003-2065-5410; Rico, Javier/0000-0003-4137-1134; Lopez Moya,
Marcos/0000-0002-8791-7908; Antoranz, Pedro/0000-0002-3015-3601;
Miranda, Jose Miguel/0000-0002-1472-9690; GAug,
Markus/0000-0001-8442-7877; Font, Lluis/0000-0003-2109-5961; Moralejo
Olaizola, Abelardo/0000-0002-1344-9080; Sokolovsky,
Kirill/0000-0001-5991-6863
FU German BMBF; MPG; Italian INFN; Swiss National Fund SNF; Spanish MICINN;
CPAN [CSD2007-00042]; MultiDark [CSD2009-00064]; Academy of Finland
[127740]; DFG Cluster of Excellence "Origin and Structure of the
Universe"; DFG Collaborative Research Centers [SFB823/C4, SFB876/C3];
Polish MNiSzW [745/N-HESS-MAGIC/2010/0]; Italian Space Agency (ASI);
Italian Institute of Astrophysics (INAF); Italian Institute of Nuclear
Physics (INFN); ASI [I/089/06/2, I/042/10/0]
FX We would like to thank the anonymous referee for constructive comments.
The MAGIC Collaboration would like to thank the Instituto de Astrofisica
de Canarias for the excellent working conditions at the Observatorio del
Roque de los Muchachos in La Palma. The support of the German BMBF and
MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish
MICINN is gratefully acknowledged. This work was also supported by the
CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish
Consolider-Ingenio 2010 programme, by grant 127740 of the Academy of
Finland, by the DFG Cluster of Excellence "Origin and Structure of the
Universe", by the DFG Collaborative Research Centers SFB823/C4 and
SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. The
AGILE Mission is funded by the Italian Space Agency (ASI), with
scientific and programmatic participation by the Italian Institute of
Astrophysics (INAF) and the Italian Institute of Nuclear Physics (INFN).
Research partially supported through the ASI grants no. I/089/06/2 and
I/042/10/0. The Fermi-LAT Collaboration acknowledges support from a
number of agencies and institutes for both development and the operation
of the LAT as well as scientific data analysis. These include NASA and
DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and
INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg
Foundation, the Swedish Research Council and the National Space Board in
Sweden. Additional support from INAF in Italy and CNES in France for
science analysis during the operations phase is also gratefully
acknowledged. We gratefully acknowledge the entire Swift team, the duty
scientists and science planners for the dedicated support, making these
observations possible. This research has made use of the XRT Data
Analysis Software (XRTDAS) developed under the responsibility of the ASI
Science Data Center (ASDC), Italy. This research is partly based on
observations with the 100-m telescope of the MPIfR (Max-Planck-Institut
fur Radioastronomie) at Effelsberg and has made use of observations with
the IRAM 30-m telescope. IRAM is supported by INSU/CNRS (France), MPG
(Germany) and IGN (Spain). The Metsahovi team acknowledges the support
from the Academy of Finland to our observing projects (numbers 212656,
210338, 121148, and others). This research has made use of data from the
MOJAVE database that is maintained by the MOJAVE team (Lister et al.
2009a). The MOJAVE project is supported under NASA-Fermi grant
NNX08AV67G. The VLBA is a facility of the National Science Foundation
operated by the National Radio Astronomy Observatory under cooperative
agreement with Associated Universities, Inc. This work made use of the
Swinburne University of Technology software correlator, developed as
part of the Australian Major National Research Facilities Programme and
operated under licence. RATAN-600 operations were carried out with the
financial support of the Ministry of Education and Science of the
Russian Federation (contracts 16.518.11.7062 and 16.552.11.7028). This
publication makes use of data products from the Two Micron All Sky
Survey, 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 research has made use of
NASA's Astrophysics Data System. Part of this work is based on archival
data, software or on-line services provided by the ASI Science Data
Center (ASDC).; 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. This research has made
use of SAOImage DS9, developed by Smithsonian Astrophysical Observatory.
This research has made use of the SIMBAD database, operated at CDS,
Strasbourg, France. Y. A. K., Y. Y. K., and K. V. S. were supported in
part by the Russian Foundation for Basic Research (projects 11-02-00368,
12-02-33101), the basic research program "Active processes in galactic
and extragalactic objects" of the Physical Sciences Division of the
Russian Academy of Sciences, and the Ministry of Education and Science
of the Russian Federation (agreement No. 8405). Y. Y. K. was also
supported by the Dynasty Foundation.
NR 125
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FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2013
VL 556
AR UNSP A67
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SC Astronomy & Astrophysics
GA 211GH
UT WOS:000323893500067
ER
PT J
AU Ducci, L
Romano, P
Esposito, P
Bozzo, E
Krimm, HA
Vercellone, S
Mangano, V
Kennea, JA
AF Ducci, L.
Romano, P.
Esposito, P.
Bozzo, E.
Krimm, H. A.
Vercellone, S.
Mangano, V.
Kennea, J. A.
TI Swift/XRT orbital monitoring of the candidate supergiant fast X-ray
transient IGR J17354-3255
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: binaries; stars: individual: IGR J17354-3255
ID VELA X-1; NEUTRON-STAR; BINARIES; MASS; WINDS; TELESCOPE; CATALOG;
STATISTICS; PARAMETERS; OUTBURSTS
AB We report on the Swift/X-ray Telescope (XRT) monitoring of the field of view around the candidate supergiant fast X-ray transient (SFXT) IGR J17354-3255, which is positionally associated with the AGILE/GRID gamma-ray transient AGL J1734-3310. Our observations, which cover 11 days for a total on-source exposure of similar to 24 ks, span 1.2 orbital periods (P-orb = 8.4474 d) and are the first sensitive monitoring of this source in the soft X-rays. These new data allow us to exploit the timing variability properties of the sources in the field to unambiguously identify the soft X-ray counterpart of IGR J17354-3255. The soft X-ray light curve shows a moderate orbital modulation and a dip. We investigated the nature of the dip by comparing the X-ray light curve with the prediction of the Bondi-Hoyle-Lyttleton accretion theory, assuming both spherical and nonspherical symmetry of the outflow from the donor star. We found that the dip cannot be explained with the X-ray orbital modulation. We propose that an eclipse or the onset of a gated mechanism is the most likely explanation for the observed light curve.
C1 [Ducci, L.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Romano, P.; Vercellone, S.; Mangano, V.] Ist Astrofis Spaziale & Fis Cosm Palermo, INAF, I-90146 Palermo, Italy.
[Esposito, P.] Ist Astrofis Spaziale & Fis Cosm Milano, INAF, I-20133 Milan, Italy.
[Bozzo, E.] Univ Geneva, Data Ctr Astrophys, ISDC, CH-1290 Versoix, Switzerland.
[Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krimm, H. A.] Univ Space Res Assoc, Columbia, MD USA.
[Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Ducci, L (reprint author), Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
EM ducci@astro.uni-tuebingen.de
OI Vercellone, Stefano/0000-0003-1163-1396; Esposito,
Paolo/0000-0003-4849-5092
FU Deutsche Forschungsgemeinschaft [SA 2131/1]; [ASI-INAFI/004/11/0]
FX We thank the anomymous referee for constructive comments which helped to
improve the paper. We thank the Swift team duty scientists and science
planners. We also thank the remainder of the Swift XRT and BAT teams, S.
D. Barthelmy, J. A. Nousek, and D. N. Burrows in particular, for their
invaluable help and support of the SFXT project as a whole. We thank P.
A. Evans and C. Ferrigno for helpful discussions. We acknowledge
financial contribution from the contract ASI-INAFI/004/11/0. L. D.
acknowledges support by the Deutsche Forschungsgemeinschaft through the
Emmy Noether Research Grant SA 2131/1. This work made use of the results
of the Swift/BAT hard X-ray transient monitor:
http://swift.gsfc.nasa.gov/docs/swift/results/transients/
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J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2013
VL 556
AR UNSP A72
DI 10.1051/0004-6361/201321635
PG 8
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SC Astronomy & Astrophysics
GA 211GH
UT WOS:000323893500072
ER
PT J
AU Iserlohe, C
Krabbe, A
Larkin, JE
Barczys, M
McElwain, MW
Quirrenbach, A
Weiss, J
Wright, SA
AF Iserlohe, C.
Krabbe, A.
Larkin, J. E.
Barczys, M.
McElwain, M. W.
Quirrenbach, A.
Weiss, J.
Wright, S. A.
TI Near-infrared imaging spectroscopy of the inner few arcseconds of NGC
4151 with OSIRIS at Keck
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; galaxies: individual: NGC 4151
ID NARROW-LINE REGION; SEYFERT-GALAXY NGC-4151; ACTIVE GALACTIC NUCLEI;
SPECTROGRAPH ECHELLE OBSERVATIONS; MOLECULAR-HYDROGEN EMISSION;
INTRINSIC ABSORPTION-LINES; HUBBLE-SPACE-TELESCOPE; FIELD SPECTROGRAPH;
GEMINI NIFS; H-I
AB We present H-and K-band data from the inner arcsecond of the Seyfert 1.5 galaxy NGC 4151 obtained with the adaptive-optics-assisted near-infrared-imaging field spectrograph OSIRIS at the Keck Observatory. The angular resolution is about a few parsecs on-site and thus competes easily with optical images taken previously with the Hubble Space Telescope. We present the morphology and dynamics of most species detected but focus on the morphology and dynamics of the narrow line region (as traced by emission of [FeII]lambda 1.644 mu m), the interplay between plasma ejected from the nucleus (as traced by 21 cm continuum radio data) and hot H-2 gas and characterize the detected nuclear HeI lambda 2.058 mu m absorption feature as a narrow absorption line (NAL) phenomenon. The emission from the narrow line region (NLR) as traced by [FeII] reveals a biconical morphology and we compare the measured dynamics in the [FeII] emission line with models that propose acceleration of gas in the NLR and simple ejection of gas into the NLR. In the inner 2.5 arcsec the acceleration model reveals a better fit to our data than the ejection model. We also see evidence that the jet very locally enhances emission in [FeII] at certain positions in our field-of-view such that we were able to distinct the kinematics of these clouds from clouds generally accelerated in the NLR. Further, the radio jet is aligned with the bicone surface rather than the bicone axis such that we assume that the jet is not the dominant mechanism responsible for driving the kinematics of clouds in the NLR. The hot H2 gas is thermal with a temperature of about 1700 K. We observe a remarkable correlation between individual H2 clouds at systemic velocity with the 21 cm continuum radio jet. We propose that the radio jet is at least partially embedded in the galactic disk of NGC 4151 such that deviations from a linear radio structure are invoked by interactions of jet plasma with H2 clouds that are moving into the path of the jet because of rotation of the galactic disk of NGC 4151. Additionally, we observe a correlation of the jet as traced by the radio data, with gas as traced in Br gamma. and H-2, at velocities between systemic and +/- 200 km s(-1) at several locations along the path of the jet. The HeI lambda 2.058 mu m line in NGC 4151 appears in emission with a blueshifted absorption component from an outflow. The emission (absorption) component has a velocity offset of 10 kms(-1) (-280 km s(-1)) with a Gaussian (Lorentzian) full-width (half-width) at half maximum of 160 km s(-1) (440 km s(-1)). The absorption component remains spatially unresolved and its kinematic measures differ from that of UV resonance absorption lines. From the amount of absorption we derive a lower limit of the HeI 2(1)S column density of 1 x 1014 cm(-2) with a covering factor along the line-of-sight of C-los similar or equal to 0.1.
C1 [Iserlohe, C.] Univ Cologne, Inst Phys, D-50937 Cologne, Germany.
[Krabbe, A.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
[Larkin, J. E.; Weiss, J.] Univ Calif Los Angeles, Div Astron, Los Angeles, CA 90095 USA.
[Barczys, M.] Univ Rochester, Laser Energet Lab, Rochester, NY 14627 USA.
[McElwain, M. W.] NASA, Exoplanets & Stellar Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Quirrenbach, A.] Heidelberg Univ, Zentrum Astron, Landessternwarte, D-69117 Heidelberg, Germany.
[Wright, S. A.] Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Iserlohe, C (reprint author), Univ Cologne, Inst Phys, Zulpicher Str 77, D-50937 Cologne, Germany.
EM ciserlohe@ph1.uni-koeln.de
OI Wright, Shelley/0000-0003-1034-8054
NR 68
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JI Astron. Astrophys.
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PY 2013
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SC Astronomy & Astrophysics
GA 211GH
UT WOS:000323893500136
ER
PT J
AU Oshagh, M
Santos, NC
Boisse, I
Boue, G
Montalto, M
Dumusque, X
Haghighipour, N
AF Oshagh, M.
Santos, N. C.
Boisse, I.
Boue, G.
Montalto, M.
Dumusque, X.
Haghighipour, N.
TI Effect of stellar spots on high-precision transit light-curve
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planets and satellites: detection; planetary systems; methods:
numerical; stars: activity; techniques: photometric
ID HUBBLE-SPACE-TELESCOPE; TIME-SERIES PHOTOMETRY; EXOPLANETARY SYSTEM;
TIMING VARIATIONS; RADIAL-VELOCITY; STARSPOTS; PLANET; STAR;
VARIABILITY; DISCOVERY
AB Stellar-activity features such as spots can complicate the determination of planetary parameters through spectroscopic and photometric observations. The overlap of a transiting planet and a stellar spot, for instance, can produce anomalies in the transit light-curves that may lead to an inaccurate estimation of the transit duration, depth, and timing. These inaccuracies can for instance affect the precise derivation of the planet radius. We present the results of a quantitative study on the effects of stellar spots on high-precision transit light-curves. We show that spot anomalies can lead to an estimate of a planet radius that is 4% smaller than the real value. Likewise, the transit duration may be estimated about 4%, longer or shorter. Depending on the size and distribution of spots, anomalies can also produce transit-timing variations (TTVs) with significant amplitudes. For instance, TTVs with signal amplitudes of 200 s can be produced when the spot is completely dark and has the size of the largest Sun spot. Our study also indicates that the smallest size of a stellar spot that still has detectable effects on a high-precision transit light-curve is around 0.03 time the stellar radius for typical Kepler Telescope precision. We also show that the strategy of including more free parameters (such as transit depth and duration) in the fitting procedure to measure the transit time of each individual transit will not produce accurate results for active stars.
C1 [Oshagh, M.; Santos, N. C.; Boisse, I.; Montalto, M.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Oshagh, M.; Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4169007 Oporto, Portugal.
[Boue, G.] Univ Chicago, Ctr Astron & Astrophys, Chicago, IL 60637 USA.
[Dumusque, X.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland.
[Haghighipour, N.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Haghighipour, N.] Univ Hawaii Manoa, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
RP Oshagh, M (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal.
EM moshagh@astro.up.pt
RI Santos, Nuno/E-9957-2011;
OI Santos, Nuno/0000-0003-4422-2919; Boisse, Isabelle/0000-0001-8388-8399;
Oshagh, Mahmoudreza/0000-0002-0715-8789; Montalto,
Marco/0000-0002-7618-8308
FU European Research Council/European Community [239953]; Fundacao para a
Ciencia e a Tecnologia (FCT) [PTDC/CTE-AST/098528/2008,
SFRH/BPD/81084/2011, SFRH/BD/51981/2012]; FCT; FCT/MCTES (Portugal);
POPH/FSE (EC); Hubble Space Telescope grant [HST-GO-12548.06-A]; NASA
Astrobiology Institute [NNA09DA77]
FX We acknowledge the support from the European Research Council/European
Community under the FP7 through Starting Grant agreement number 239953,
and by Fundacao para a Ciencia e a Tecnologia (FCT) in the form of
grants reference PTDC/CTE-AST/098528/2008, SFRH/BPD/81084/2011 and
SFRH/BD/51981/2012. NCS also acknowledges the support from FCT through
program Ciencia 2007 funded by FCT/MCTES (Portugal) and POPH/FSE (EC).
N.H. acknowledges support from the Hubble Space Telescope grant
HST-GO-12548.06-A and from the NASA Astrobiology Institute under
Cooperative Agreement NNA09DA77 at the Institute for Astronomy,
University of Hawaii.
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JI Astron. Astrophys.
PD AUG
PY 2013
VL 556
AR A19
DI 10.1051/0004-6361/201321309
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211GH
UT WOS:000323893500019
ER
PT J
AU Peter, H
Bingert, S
Klimchuk, JA
de Forest, C
Cirtain, JW
Golub, L
Winebarger, AR
Kobayashi, K
Korreck, KE
AF Peter, H.
Bingert, S.
Klimchuk, J. A.
de Forest, C.
Cirtain, J. W.
Golub, L.
Winebarger, A. R.
Kobayashi, K.
Korreck, K. E.
TI Structure of solar coronal loops: from miniature to large-scale
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: corona; magnetic fields; Sun: UV radiation; Sun: activity; methods:
data analysis
ID DYNAMICS-OBSERVATORY SDO; ACTIVE-REGION LOOPS; TRANSITION-REGION;
MAGNETIC-FIELDS; BRIGHT POINTS; COOL LOOPS; HINODE; MODEL; TRACE; SUN
AB Aims. We use new data from the High-resolution Coronal Imager (Hi-C) with its unprecedented spatial resolution of the solar corona to investigate the structure of coronal loops down to 0.2 ''.
Methods. During a rocket flight, Hi-C provided images of the solar corona in a wavelength band around 193 angstrom that is dominated by emission from Fe XII showing plasma at temperatures around 1.5 MK. We analyze part of the Hi-C field-of-view to study the smallest coronal loops observed so far and search for the possible substructuring of larger loops.
Results. We find tiny 1.5 MK loop-like structures that we interpret as miniature coronal loops. Their coronal segments above the chromosphere have a length of only about 1 Mm and a thickness of less than 200 km. They could be interpreted as the coronal signature of small flux tubes breaking through the photosphere with a footpoint distance corresponding to the diameter of a cell of granulation. We find that loops that are longer than 50 Mm have diameters of about 2 '' or 1.5 Mm, which is consistent with previous observations. However, Hi-C really resolves these loops with some 20 pixels across the loop. Even at this greatly improved spatial resolution, the large loops seem to have no visible substructure. Instead they show a smooth variation in cross-section.
Conclusions. That the large coronal loops do not show a substructure on the spatial scale of 0.1 '' per pixel implies that either the densities and temperatures are smoothly varying across these loops or it places an upper limit on the diameter of the strands the loops might be composed of. We estimate that strands that compose the 2 '' thick loop would have to be thinner than 15 km. The miniature loops we find for the first time pose a challenge to be properly understood through modeling.
C1 [Peter, H.; Bingert, S.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Klimchuk, J. A.] NASA, Heliophys Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[de Forest, C.] SW Res Inst, Instrumentat & Space Res Div, Boulder, CO 80302 USA.
[Cirtain, J. W.; Winebarger, A. R.] NASA, George C Marshall Space Flight Ctr, MSFC, Huntsville, AL 35812 USA.
[Golub, L.; Korreck, K. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA.
[Kobayashi, K.] Univ Alabama, Ctr Space & Aeronaut Res, Huntsville, AL 35812 USA.
RP Peter, H (reprint author), Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
EM peter@mps.mpg.de
RI Klimchuk, James/D-1041-2012
OI Klimchuk, James/0000-0003-2255-0305
FU NASA's Low Cost Access to Space program; Max-Planck/Princeton Center for
Plasma Physics; NASA
FX We acknowledge the High-resolution Coronal Imager instrument grant
funded by the NASA's Low Cost Access to Space program. MSFC/NASA led the
mission and partners include the Smithsonian Astrophysical Observatory
in Cambridge, Mass.; Lockheed Martin's Solar Astrophysical Laboratory in
Palo Alto, Calif.; the University of Central Lancashire in Lancashire,
England; and the Lebedev Physical Institute of the Russian Academy of
Sciences in Moscow. The AIA and HMI data used are provided courtesy of
NASA/SDO and the AIA and HMI science teams. The AIA and HMI data have
been retrieved using the German Data Center for SDO. The numerical
simulation was conducted at the High Performance Computing Center
Stuttgart (HLRS). This work was partially funded by the
Max-Planck/Princeton Center for Plasma Physics. The work of J.A.K. was
supported by the NASA Supporting Research and Technology and Guest
Investigator Programs. H.P. acknowledges stimulating discussions with
Robert Cameron and Aaron Birch. We thank the anonymous referee for
constructive comments.
NR 51
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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 AUG
PY 2013
VL 556
AR A104
DI 10.1051/0004-6361/201321826
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211GH
UT WOS:000323893500104
ER
PT J
AU Wu, R
Polehampton, ET
Etxaluze, M
Makiwa, G
Naylor, DA
Salji, C
Swinyard, BM
Ferlet, M
van der Wiel, MHD
Smith, AJ
Fulton, T
Griffin, MJ
Baluteau, JP
Benielli, D
Glenn, J
Hopwood, R
Imhof, P
Lim, T
Lu, N
Panuzzo, P
Pearson, C
Sidher, S
Valtchanov, I
AF Wu, R.
Polehampton, E. T.
Etxaluze, M.
Makiwa, G.
Naylor, D. A.
Salji, C.
Swinyard, B. M.
Ferlet, M.
van der Wiel, M. H. D.
Smith, A. J.
Fulton, T.
Griffin, M. J.
Baluteau, J. -P.
Benielli, D.
Glenn, J.
Hopwood, R.
Imhof, P.
Lim, T.
Lu, N.
Panuzzo, P.
Pearson, C.
Sidher, S.
Valtchanov, I.
TI Observing extended sources with the Herschel SPIRE Fourier Transform
Spectrometer
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE instrumentation: spectrographs; methods: analytical; methods: data
analysis; techniques: spectroscopic
ID CONTINUUM OBSERVATIONS; INTERSTELLAR-MEDIUM; STELLAR ORBITS; SAGITTARIUS
B2; SPECTRAL-LINE; BLACK-HOLE; INSTRUMENT; SPECTROSCOPY; REGION;
CALIBRATION
AB The Spectral and Photometric Imaging Receiver (SPIRE) on the European Space Agency's Herschel Space Observatory utilizes a pioneering design for its imaging spectrometer in the form of a Fourier Transform Spectrometer (FTS). The standard FTS data reduction and calibration schemes are aimed at objects with either a spatial extent that is much larger than the beam size or a source that can be approximated as a point source within the beam. However, when sources are of intermediate spatial extent, neither of these calibrations schemes is appropriate and both the spatial response of the instrument and the source's light profile must be taken into account and the coupling between them explicitly derived. To that end, we derive the necessary corrections using an observed spectrum of a fully extended source with the beam profile and considering the source's light profile. We apply the derived correction to several observations of planets and compare the corrected spectra with their spectral models to study the beam coupling efficiency of the instrument in the case of partially extended sources. We find that we can apply these correction factors for sources with angular sizes up to theta(D) similar to 17 ''. We demonstrate how the angular size of an extended source can be estimated using the difference between the subspectra observed at the overlap bandwidth of the two frequency channels in the spectrometer, at 959 < nu < 989 GHz. Using this technique on an observation of Saturn, we estimate a size of 17.2 '', which is 3% larger than its true size on the day of observation. Finally, we show the results of the correction applied on observations of a nearby galaxy, M82, and the compact core of a Galactic molecular cloud, Sgr B2.
C1 [Wu, R.; Panuzzo, P.] CEA Saclay, Irfu Serv Astrophys, CNRS, CEA DSM,Lab AIM, F-91191 Gif Sur Yvette, France.
[Polehampton, E. T.; Salji, C.; Swinyard, B. M.; Ferlet, M.; Lim, T.; Pearson, C.; Sidher, S.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England.
[Polehampton, E. T.; Makiwa, G.; Naylor, D. A.; van der Wiel, M. H. D.; Fulton, T.; Imhof, P.] Univ Lethbridge, Dept Phys & Astron, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada.
[Etxaluze, M.] Ctr Astrobiol CSIC INTA, Madrid 28850, Spain.
[Salji, C.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HA, England.
[Salji, C.] Kavli Inst Cosmol, Cambridge CB3 0HA, England.
[Salji, C.; Swinyard, B. M.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Smith, A. J.; Fulton, T.; Imhof, P.] Blue Sky Spect, Lethbridge, AB T1J 0N9, Canada.
[Griffin, M. J.] Cardiff Univ, Cardiff CF10 3AX, S Glam, Wales.
[Baluteau, J. -P.; Benielli, D.] Univ Aix Marseille, LAM, F-13388 Marseille 13, France.
[Baluteau, J. -P.; Benielli, D.] CNRS, UMR 7326, F-13388 Marseille 13, France.
[Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron, UCB 389, Boulder, CO 80303 USA.
[Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England.
[Lu, N.] NASA, Herschel Sci Ctr, IPAC, Pasadena, CA USA.
[Pearson, C.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Valtchanov, I.] ESA, Herschel Sci Ctr, European Space Astron Ctr, Villanueva De La Canada 28691, Spain.
RP Wu, R (reprint author), CEA Saclay, Irfu Serv Astrophys, CNRS, CEA DSM,Lab AIM, F-91191 Gif Sur Yvette, France.
EM ronin.wu@cea.fr
RI van der Wiel, Matthijs/M-4531-2014
OI van der Wiel, Matthijs/0000-0002-4325-3011
FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France);
ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA);
ASTROMADRID [S2009ESP-1496]; Spanish MINECO [AYA2009-07304]; Spanish
Consolider-Ingenio program [ASTROMOL: CSD2009-00038]; NSERC
FX SPIRE has been developed by a consortium of institutes led by Cardiff
University (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 (UK); and NASA (USA). R.W. would like to
thank Dr. J. Bock, F. Galliano, S. Hony, J. Kamenetzky, and, C. Wilson
for their helpful discussions and comments on this work. M.E. thanks
ASTROMADRID for funding support through the grant S2009ESP-1496, the
Spanish MINECO (grant AYA2009-07304) and the Spanish Consolider-Ingenio
program, ASTROMOL: CSD2009-00038. G.M., D.N. and M.v.d.W. acknowledge
support from NSERC.
NR 45
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U1 0
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2013
VL 556
AR A116
DI 10.1051/0004-6361/201321837
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 211GH
UT WOS:000323893500116
ER
PT J
AU West, TO
Brown, ME
Duren, RM
Ogle, SM
Moss, RH
AF West, Tristram O.
Brown, Molly E.
Duren, Riley M.
Ogle, Stephen M.
Moss, Richard H.
TI Definition, capabilities and components of a terrestrial carbon
monitoring system
SO CARBON MANAGEMENT
LA English
DT Article
ID UNITED-STATES; WOOD HARVEST; LAND-USE; INVENTORY; CLIMATE; UNCERTAINTY;
RESOLUTION; FLUXES; MODEL; CYCLE
AB Research efforts for effectively and consistently monitoring terrestrial carbon are increasing in number. As such, there is a need to define carbon monitoring and how it relates to carbon cycle science and carbon management. There is also a need to identify capabilities of a carbon monitoring system and the system components needed to develop the capabilities. Capabilities that enable the effective application of a carbon monitoring system for monitoring and management purposes may include: reconciling carbon stocks and fluxes, developing consistency across spatial and temporal scales, tracking horizontal movement of carbon, attribution of emissions to originating sources, cross-sectoral accounting, uncertainty quantification, redundancy and policy relevance. Focused research is needed to integrate these capabilities for sustained estimates of carbon stocks and fluxes. Additionally, if monitoring is intended to inform management decisions, management priorities should be considered prior to development of a monitoring system.
C1 [West, Tristram O.; Moss, Richard H.] Pacific NW Natl Lab, Joint Global Change Res Inst, College Pk, MD 20740 USA.
[Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Duren, Riley M.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Duren, Riley M.] CALTECH, Pasadena, CA 91109 USA.
[Ogle, Stephen M.] Colorado State Univ, Nat Resource Ecol Lab, Ft Collins, CO 80523 USA.
RP West, TO (reprint author), Pacific NW Natl Lab, Joint Global Change Res Inst, 5825 Univ Res Court, College Pk, MD 20740 USA.
EM tristram.west@pnnl.gov
RI West, Tristram/C-5699-2013; Brown, Molly/M-5146-2013; Brown,
Molly/E-2724-2010;
OI West, Tristram/0000-0001-7859-0125; Brown, Molly/0000-0001-7384-3314;
Brown, Molly/0000-0001-7384-3314; Ogle, Stephen/0000-0003-1899-7446;
Moss, Richard/0000-0001-5005-0063
FU National Aeronautics and Space Administration under Carbon Monitoring
System Phase 2 Project [NNH12AU35I]; Jet Propulsion Laboratory, a
division of the California Institute of Technology
FX Support for TO West is from the National Aeronautics and Space
Administration under Carbon Monitoring System Phase 2 Project
#NNH12AU35I. Support for Rill Duren is from the Jet Propulsion
Laboratory, a division of the California Institute of Technology under
contract to the National Aeronautics and Space Administration. The
authors have no other relevant affiliations or financial involvement
with any organization or entity with a financial interest in or
financial conflict with the subject matter or materials discussed in the
manuscript apart from those disclosed.
NR 59
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U1 0
U2 16
PU FUTURE SCI LTD
PI LONDON
PA UNITED HOUSE, 2 ALBERT PL, LONDON, N3 1QB, ENGLAND
SN 1758-3004
J9 CARBON MANAG
JI Carbon Manag.
PD AUG
PY 2013
VL 4
IS 4
BP 413
EP 422
DI 10.4155/CMT.13.36
PG 10
WC Environmental Sciences; Environmental Studies
SC Environmental Sciences & Ecology
GA 198RR
UT WOS:000322940500015
ER
PT J
AU Rim, T
Kim, K
Kim, S
Baek, CK
Meyyappan, M
Jeong, YH
Lee, JS
AF Rim, Taiuk
Kim, Kihyun
Kim, Sungho
Baek, Chang-Ki
Meyyappan, Meyya
Jeong, Yoon-Ha
Lee, Jeong-Soo
TI Improved Electrical Characteristics of Honeycomb Nanowire ISFETs
SO IEEE ELECTRON DEVICE LETTERS
LA English
DT Article
DE Honeycomb nanowire structure (HCNW); ion-sensitive field-effect
transistor (ISFET); pH sensing; silicon nanowire
ID FIELD-EFFECT TRANSISTORS; IMMUNODETECTION; ELECTRODE
AB Ion-sensitive field-effect transistors (ISFETs) with a honeycomb nanowire (HCNW) structure have been fabricated on a silicon-on-insulator wafer. The HCNW ISFET shows lower threshold voltage, lower subthreshold swing, higher drain current, and lower variability than the conventional nanowire device. Improved electrical characteristics are mainly due to the increased effective channel width and enhanced current drivability. The HCNW structure also exhibits improved current sensitivity in its pH response. These results suggest that the HCNW structure is promising for enhancing device performance and realizing sensors with high sensitivity.
C1 [Rim, Taiuk; Kim, Kihyun; Jeong, Yoon-Ha; Lee, Jeong-Soo] Pohang Univ Sci & Technol, Dept Elect Engn, Pohang 790784, South Korea.
[Baek, Chang-Ki; Jeong, Yoon-Ha] Pohang Univ Sci & Technol, Dept Creat IT Engn, Pohang 790784, South Korea.
[Meyyappan, Meyya] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Meyyappan, Meyya; Jeong, Yoon-Ha; Lee, Jeong-Soo] Pohang Univ Sci & Technol, Div IT Convers Engn, Pohang 790784, South Korea.
RP Rim, T (reprint author), Pohang Univ Sci & Technol, Dept Elect Engn, Pohang 790784, South Korea.
EM hacle@postech.ac.kr; baekck@postech.ac.kr; m.meyyappan@nasa.gov;
yhjeong@postech.ac.kr; ljs6951@postech.ac.kr
FU WCU program [R31-10100]; NIPA [NIPA-2013-H0203-13-1001]
FX Manuscript received May 1, 2013; revised May 16, 2013; accepted May 27,
2013. Date of publication July 3, 2013; date of current version July 22,
2013. This work was supported in part by the WCU program under Grant
R31-10100 and the "IT Consilience Creative Program" of the NIPA under
Grant NIPA-2013-H0203-13-1001. The review of this letter was arranged by
Editor C. V. Mouli.
NR 11
TC 5
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U1 2
U2 21
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0741-3106
J9 IEEE ELECTR DEVICE L
JI IEEE Electron Device Lett.
PD AUG
PY 2013
VL 34
IS 8
BP 1059
EP 1061
DI 10.1109/LED.2013.2265391
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA 211MK
UT WOS:000323911800042
ER
PT J
AU Bursalioglu, OY
Caire, G
Divsalar, D
AF Bursalioglu, O. Y.
Caire, G.
Divsalar, D.
TI Joint Source-Channel Coding for Deep-Space Image Transmission using
Rateless Codes
SO IEEE TRANSACTIONS ON COMMUNICATIONS
LA English
DT Article
DE Joint source-channel coding; deep-space communications; image coding;
raptor codes
ID RAPTOR CODES; COMPRESSION
AB A new coding scheme for image transmission over noisy channel is proposed. Similar to standard image compression, the scheme includes a linear transform followed by successive refinement scalar quantization. Unlike conventional schemes, though, in the proposed system the quantized transform coefficients are linearly mapped into channel symbols using systematic linear encoders. This fixed-to-fixed length "linear index coding" approach avoids the use of an explicit entropy coding stage (e.g., arithmetic or Huffman coding), which is typically fragile to channel post-decoding residual errors. We use linear codes over GF(4), which are particularly suited for this application, since they are matched to the dead-zone quantizer symbol alphabet and to the QPSK modulation used on the deep-space communication channel. We optimize the proposed system where the linear codes are systematic Raptor codes over GF(4). The rateless property of Raptor encoders allows to implement a "continuum" of coding rates, in order to accurately match the channel coding rate to the transmission channel capacity and to the quantized source entropy rate for each transform subband and refinement level. Comparisons are provided with respect to the concatenation of state-of-the-art image coding and channel coding schemes used by Jet Propulsion Laboratories (JPL) for the Mars Exploration Rover (MER) Mission.
C1 [Bursalioglu, O. Y.] Docomo Innovat Inc, Area Wireless Commun MIMO Tech & LTE A Enhancemen, Palo Alto, CA USA.
[Caire, G.] Univ So Calif, Ming Hsieh Dept Elect Engn, Viterbi Sch Engn, Los Angeles, CA USA.
[Divsalar, D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Bursalioglu, OY (reprint author), Docomo Innovat Inc, Area Wireless Commun MIMO Tech & LTE A Enhancemen, Palo Alto, CA USA.
EM ozgun.bu@gmail.com
FU NASA/JPL/DRDF/SURP Program; NASA
FX This research in part was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. The work
by the University of Southern California, and JPL was funded through the
NASA/JPL/DRDF/SURP Program.
NR 36
TC 6
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U1 1
U2 12
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0090-6778
J9 IEEE T COMMUN
JI IEEE Trans. Commun.
PD AUG
PY 2013
VL 61
IS 8
BP 3448
EP 3461
DI 10.1109/TCOMM.2013.061913.120747
PG 14
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 208AP
UT WOS:000323647500034
ER
PT J
AU Goodwin, TJ
McCarthy, M
Osterrieder, N
Cohrs, RJ
Kaufer, BB
AF Goodwin, Thomas J.
McCarthy, Maureen
Osterrieder, Nikolaus
Cohrs, Randall J.
Kaufer, Benedikt B.
TI Three-Dimensional Normal Human Neural Progenitor Tissue-Like Assemblies:
A Model of Persistent Varicella-Zoster Virus Infection
SO PLOS PATHOGENS
LA English
DT Article
ID HUMAN TRIGEMINAL GANGLIA; LATENCY-ASSOCIATED TRANSCRIPT; MEMORY EFFECTOR
PHENOTYPE; EMBRYONIC STEM-CELLS; HUMAN-MELANOMA CELLS; DORSAL-ROOT
GANGLIA; EXPANDED T-CELLS; IN-VIVO; CHROMOSOME-ABERRATIONS;
HUMAN-LYMPHOCYTES
AB Varicella-zoster virus (VZV) is a neurotropic human alphaherpesvirus that causes varicella upon primary infection, establishes latency in multiple ganglionic neurons, and can reactivate to cause zoster. Live attenuated VZV vaccines are available; however, they can also establish latent infections and reactivate. Studies of VZV latency have been limited to the analyses of human ganglia removed at autopsy, as the virus is strictly a human pathogen. Recently, terminally differentiated human neurons have received much attention as a means to study the interaction between VZV and human neurons; however, the short life-span of these cells in culture has limited their application. Herein, we describe the construction of a model of normal human neural progenitor cells (NHNP) in tissue-like assemblies (TLAs), which can be successfully maintained for at least 180 days in three-dimensional (3D) culture, and exhibit an expression profile similar to that of human trigeminal ganglia. Infection of NHNP TLAs with cell-free VZV resulted in a persistent infection that was maintained for three months, during which the virus genome remained stable. Immediate-early, early and late VZV genes were transcribed, and low-levels of infectious VZV were recurrently detected in the culture supernatant. Our data suggest that NHNP TLAs are an effective system to investigate long-term interactions of VZV with complex assemblies of human neuronal cells.
C1 [Goodwin, Thomas J.; McCarthy, Maureen] NASA Johnson Space Ctr, Dis Modeling Tissue Analogues Lab, Houston, TX USA.
[Osterrieder, Nikolaus; Kaufer, Benedikt B.] Free Univ Berlin, Inst Virol, Berlin, Germany.
[Cohrs, Randall J.] Univ Colorado, Sch Med, Dept Neurol, Aurora, CO USA.
RP Goodwin, TJ (reprint author), NASA Johnson Space Ctr, Dis Modeling Tissue Analogues Lab, Houston, TX USA.
EM thomas.j.goodwin@nasa.gov; Randall.Cohrs@ucdenver.edu;
b.kaufer@fu-berlin.de
FU NASA Human Research Program/Rapid Operational Investigation grant;
Public Health Service [AG032958]; National Institutes of Health NIH)
[AI061412]
FX This work was supported by a NASA Human Research Program/Rapid
Operational Investigation grant to TJG, Public Health Service grants
AG032958 to RJC, and a grant from the National Institutes of Health NIH)
AI061412 to NO. The funders had no role in study design, data collection
and analysis, decision to publish, or preparation of the manuscript.
NR 87
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U1 3
U2 8
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1553-7374
J9 PLOS PATHOG
JI PLoS Pathog.
PD AUG
PY 2013
VL 9
IS 8
AR e1003512
DI 10.1371/journal.ppat.1003512
PG 12
WC Microbiology; Parasitology; Virology
SC Microbiology; Parasitology; Virology
GA 211EQ
UT WOS:000323888200016
PM 23935496
ER
PT J
AU Righter, K
AF Righter, Kevin
TI New constraints on the size of chondrite parent bodies
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Chondrite; eclogite; pre-solar; chondrule; inclusion; organics
ID CARBONACEOUS CHONDRITES; AMINO-ACIDS; MET 00426; QUE 99177; METEORITES;
GRAINS
AB Carbonaceous chondrites make up a majority of asteroids in the asteroid belt, yet are relatively rare in meteorite collections at approximately 5%. The rare CR carbonaceous chondrites are providing a wealth of new discoveries including (1) abundant organic compounds required for biochemical processes, (2) pre-solar mineral grains that hold isotopic records of stellar processes, (3) inclusions, chondrules, and chondrule rims that contain information about the early Solar System, (4) hydrous minerals that formed during aqueous alteration of the matrix and other components, and (5) foreign clasts that formed at slightly higher pressures than normally expected in the early Solar System. All of these discoveries suggest these carbonaceous meteorites will continue providing new information and help to revise our understanding of the broad range of conditions existing in the early Solar System.
C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Righter, K (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mailcode KT, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
NR 16
TC 1
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U1 0
U2 8
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
J9 AM MINERAL
JI Am. Miner.
PD AUG-SEP
PY 2013
VL 98
IS 8-9
BP 1379
EP 1380
DI 10.2138/am.2013.4555
PG 2
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 207FJ
UT WOS:000323584000002
ER
PT J
AU Nguyen, TV
Nosratinia, A
Divsalar, D
AF Thuy Van Nguyen
Nosratinia, Aria
Divsalar, Dariush
TI Rate-Compatible Protograph-Based LDPC Codes for Inter-Symbol
Interference Channels
SO IEEE COMMUNICATIONS LETTERS
LA English
DT Article
DE LPDC; rate-compatible; protograph; intersymbol interference
ID PARTIAL-RESPONSE CHANNELS; DESIGN; BOUNDS
AB This letter produces a family of rate-compatible protograph-based LDPC codes approaching the independent and uniformly distributed (i.u.d.) capacity of inter-symbol interference (ISI) channels. This problem is highly nontrivial due to the joint design of structured (protograph-based) LDPC codes and the state structure of ISI channels. We describe a method to design nested high-rate protograph codes by adding variable nodes to the protograph of a lower rate code. We then design a family of rate-compatible protograph codes using the extension method. The resulting protograph codes have iterative decoding thresholds close to the i.u.d. capacity. Our results are supported by numerical simulations.
C1 [Thuy Van Nguyen; Nosratinia, Aria] Univ Texas Dallas, Dept Elect Engn, Richardson, TX 75083 USA.
[Divsalar, Dariush] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nguyen, TV (reprint author), Univ Texas Dallas, Dept Elect Engn, Richardson, TX 75083 USA.
EM nvanthuy@utdallas.edu; aria@utdallas.edu; Dar-iush.Divsalar@jpl.nasa.gov
OI Nosratinia, Aria/0000-0002-3751-0165
FU NASA
FX This research was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA.
NR 15
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U1 0
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1089-7798
J9 IEEE COMMUN LETT
JI IEEE Commun. Lett.
PD AUG
PY 2013
VL 17
IS 8
BP 1632
EP 1635
DI 10.1109/LCOMM.2013.060513.130498
PG 4
WC Telecommunications
SC Telecommunications
GA 206HI
UT WOS:000323509300037
ER
PT J
AU D'Souza, S
Hsiao, F
Tang, A
Tam, SW
Berenguer, R
Chang, MCF
AF D'Souza, Sandeep
Hsiao, Frank
Tang, Adrian
Tam, Sai-Wang
Berenguer, Roc
Chang, Mau-Chung Frank
TI A 10-Bit 2-GS/s DAC-DDFS-IQ-Controller Baseband Enabling a Self-Healing
60-GHz Radio-on-Chip
SO IEEE TRANSACTIONS ON CIRCUITS AND SYSTEMS II-EXPRESS BRIEFS
LA English
DT Article
DE Digital-to-analog converter (DAC); direct digital frequency synthesizer
(DDFS); image suppression; millimeter wave; OIM3; P-1dB; self-healing;
transmitter (TX)
ID DIGITAL FREQUENCY-SYNTHESIZER; CMOS; LINEARIZATION; AMPLIFIER
AB A 10-bit 2-GS/s mixed-signal baseband (BB) circuit, which enables a self-healing 60-GHz 4-Gb/s radio-on-chip implemented in a 65-nm complementary metal-oxide semiconductor, is described. The BB circuit autonomously senses and optimizes transmitter (TX) P-1dB, OIM3, and image suppression, reducing the yield loss because of process variations. On-chip test tones are generated using a 10-bit 2-GS/s current-steering digital-to-analog converter (DAC) and direct digital frequency synthesizer (DDFS). Using the generated test tones, the aforementioned impairments are measured by an envelope detector at the power amplifier output. Based on this information, the programmable digital IQ phase amplitude and offset controller (IQ_CTRL) in the BB circuit improves the TX image suppression from -32.4 to -42.6 dBc, and digital control signals generated by the on-chip self-healing controller heal the TX P-1dB and OIM3 from 9.5 to 13.2 dBm and from -32.5 to -40 dBc, respectively. In terms of achieving the target specifications, namely, TX image suppression < -40 dBc, OIM3 < -40 dBc, and P-1dB > 10 dBm, healing increases yield on ten dies from 0% to 100%. The BB circuit consumes only 49 mW, of which 37 mW comes from the DACs and 12 mW from the DDFS and the IQ_CTRL.
C1 [D'Souza, Sandeep] Semtech Corp, Redondo Beach, CA 90277 USA.
[Hsiao, Frank; Chang, Mau-Chung Frank] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA.
[Tang, Adrian] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tam, Sai-Wang] Marvell Semicond, Santa Clara, CA 95054 USA.
[Berenguer, Roc] Univ Navarra, Pamplona 31009, Spain.
RP D'Souza, S (reprint author), Semtech Corp, Redondo Beach, CA 90277 USA.
EM sdsouza@semtech.com; fhsiao@ucla.edu; Adrian.J.Tang@jpl.nasa.gov;
Roccotam@marvell.com; rberenguer@ceit.es; mfchang@ee.ucla.edu
RI Berenguer, Roc/L-8970-2014
OI Berenguer, Roc/0000-0003-0313-7152
FU Defense Advanced Research Projects Agency/U.S. Navy [N66001-09-1-2030]
FX Manuscript received January 2, 2013; revised March 11, 2013; accepted
April 29, 2013. Date of publication July 4, 2013; date of current
version August 10, 2013. This work was supported in part by Defense
Advanced Research Projects Agency/U.S. Navy Grant N66001-09-1-2030. This
brief was recommended by Associate Editor A. Bevilacqua.
NR 11
TC 3
Z9 3
U1 1
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1549-7747
EI 1558-3791
J9 IEEE T CIRCUITS-II
JI IEEE Trans. Circuits Syst. II-Express Briefs
PD AUG
PY 2013
VL 60
IS 8
BP 457
EP 461
DI 10.1109/TCSII.2013.2268325
PG 5
WC Engineering, Electrical & Electronic
SC Engineering
GA 206JJ
UT WOS:000323515800001
ER
PT J
AU Dodds, NA
Hooten, NC
Reed, RA
Schrimpf, RD
Warner, JH
Roche, NJH
McMorrow, D
Buchner, S
Jordan, S
Pellish, JA
Bennett, WG
Gaspard, NJ
King, MP
AF Dodds, N. A.
Hooten, N. C.
Reed, R. A.
Schrimpf, R. D.
Warner, J. H.
Roche, N. J. -H.
McMorrow, D.
Buchner, S.
Jordan, S.
Pellish, J. A.
Bennett, W. G.
Gaspard, N. J.
King, M. P.
TI SEL-Sensitive Area Mapping and the Effects of Reflection and Diffraction
From Metal Lines on Laser SEE Testing
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT European Conference on Radiation and its Effects on Components and
Systems (RADECS)
CY SEP 24-28, 2012
CL Biarritz, FRANCE
SP Univ Bordeaux, IMS Labs, RADECS Org, IEEE, Nucl & Plasma Sci Soc (NPSS), French Minist Higher Educ & Res, Conseil Reg Aquitaine, French Natl Ctr Sci Res (CNRS), Univ Bordeaux
DE Laser testing; sensitive volume; single-event latchup; single-photon
absorption (SPA); two-photon absorption (TPA)
ID PARTICLE-INDUCED LATCHUP; CMOS TEST STRUCTURES; CHARGE COLLECTION;
2-PHOTON ABSORPTION; CARRIER GENERATION; PULSED-LASER; SINGLE; DEVICES;
TECHNOLOGY
AB Laser and heavy-ion data reveal the areas and shapes of single-event latchup (SEL)-sensitive regions in CMOS test structures and their positions relative to the affected p-n-p-n paths. Contrary to previous two-dimensional studies, this three-dimensional study shows that the position of maximum SEL sensitivity in these structures is not centered on a p-n-p-n region, but between two neighboring p-n-p-n regions, suggesting that synergistic triggering increases SEL sensitivity.
The SEL-sensitivity maps suggest that laser light scattered from metal lines toward the silicon can contribute to the SEE response, for both back-side-incident two-photon absorption and front-side-incident single-photon absorption laser tests. We describe the metallization configurations and laser pulse energies for which reflected and/or diffracted laser light may contribute to the single-event effect (SEE) response.
C1 [Dodds, N. A.; Hooten, N. C.; Reed, R. A.; Schrimpf, R. D.; Bennett, W. G.; Gaspard, N. J.; King, M. P.] Vanderbilt Univ, Nashville, TN 37203 USA.
[Warner, J. H.; Roche, N. J. -H.; McMorrow, D.; Buchner, S.] Naval Res Lab, Washington, DC 20375 USA.
[Jordan, S.] Jazz Semicond, Newport Beach, CA 92660 USA.
[Pellish, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Dodds, NA (reprint author), Sandia Natl Labs, Albuquerque, NM 87123 USA.
EM nadodds@sandia.gov
RI Schrimpf, Ronald/L-5549-2013
OI Schrimpf, Ronald/0000-0001-7419-2701
NR 30
TC 7
Z9 8
U1 1
U2 14
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD AUG
PY 2013
VL 60
IS 4
BP 2550
EP 2558
DI 10.1109/TNS.2013.2246189
PN 1
PG 9
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA 205NJ
UT WOS:000323450700026
ER
PT J
AU Tsiligiannis, G
Dilillo, L
Bosio, A
Girard, P
Todri, A
Virazel, A
McClure, SS
Touboul, AD
Wrobel, F
Saigne, F
AF Tsiligiannis, G.
Dilillo, L.
Bosio, A.
Girard, P.
Todri, A.
Virazel, A.
McClure, S. S.
Touboul, A. D.
Wrobel, F.
Saigne, F.
TI Testing a Commercial MRAM Under Neutron and Alpha Radiation in Dynamic
Mode
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT European Conference on Radiation and its Effects on Components and
Systems (RADECS)
CY SEP 24-28, 2012
CL Biarritz, FRANCE
SP Univ Bordeaux, IMS Labs, RADECS Org, IEEE, Nucl & Plasma Sci Soc, French Minist Higher Educ & Res, Conseil Reg Aquitaine, French Natl Ctr Sci Res (CNRS), Univ Bordeaux
DE Alpha particles; neutron; radiation; soft errors; Toggle MRAM
AB Academic and industrial research interest in terrestrial radiation effects of electronic devices has expanded over the last years from avionics and military applications to commercial applications as well. At the same time, the need for faster and more reliable memories has given growth to new memory technologies such as Magnetic (magneto-resistive) Random Access Memories (MRAM), a promising new non-volatile memory technology that will probably replace in the future the current SRAM and FLASH based memories. In this paper, we evaluate the soft error resilience of a commercial toggle MRAM in static and dynamic test mode, under neutron radiation with energies of 25, 50 and 80 MeV as well as under a Californium (Cf-252) alpha source.
C1 [Tsiligiannis, G.; Dilillo, L.; Bosio, A.; Girard, P.; Todri, A.; Virazel, A.] Univ Montpellier 2, LIRMM, CNRS, F-34095 Montpellier 5, France.
[McClure, S. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Touboul, A. D.; Wrobel, F.; Saigne, F.] Univ Montpellier 2, Inst Elect Sud, CNRS, F-34095 Montpellier 5, France.
RP Tsiligiannis, G (reprint author), Univ Montpellier 2, LIRMM, CNRS, F-34095 Montpellier 5, France.
EM tsiligiann@lirmm.fr; dilillo@lirmm.fr; bosio@lirmm.fr; girard@lirmm.fr;
todri@lirmm.fr; virazel@lirmm.fr; steven.s.mcclure@jpl.nasa.gov;
antoine.touboul@ies.univ-montp2.fr; fred-eric.wrobel@ies.univ-montp2.fr;
frederic.saigne@ies.univ-montp2.fr
RI Todri-Sanial, Aida/M-5156-2013
OI Todri-Sanial, Aida/0000-0001-8573-2910
NR 15
TC 5
Z9 5
U1 1
U2 8
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 AUG
PY 2013
VL 60
IS 4
BP 2617
EP 2622
DI 10.1109/TNS.2013.2239311
PN 1
PG 6
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA 205NJ
UT WOS:000323450700035
ER
PT J
AU Berg, M
Friendlich, M
Kim, H
Seidlick, C
LaBel, K
Ladbury, R
Pellish, J
AF Berg, Melanie
Friendlich, Mark
Kim, Hak
Seidlick, Christina
LaBel, Kenneth
Ladbury, Ray
Pellish, Jonathan
TI Characterizing the Effects of Single Event Upsets on Synchronous Data
Paths
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT European Conference on Radiation and its Effects on Components and
Systems (RADECS)
CY SEP 24-28, 2012
CL Biarritz, FRANCE
SP Univ Bordeaux, IMS Labs, RADECS Org, IEEE, Nucl & Plasma Sci Soc (NPSS), French Minist Higher Educ & Res, Conseil Reg Aquitaine, French Natl Ctr Sci Res (CNRS), Univ Bordeaux
DE Error prediction; mitigation; single event effects; synchronous design
ID PROPAGATION
AB We present a Single Event Upset (SEU) model with supporting data demonstrating frequency effects that deviate from conventional theory. The model emphasizes design topology versus circuit-element contributions to SEU cross sections.
C1 [Berg, Melanie; Friendlich, Mark; Kim, Hak; Seidlick, Christina] MEI Technol, Greenbelt, MD 20771 USA.
[LaBel, Kenneth; Ladbury, Ray; Pellish, Jonathan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Berg, M (reprint author), MEI Technol, Greenbelt, MD 20771 USA.
EM melanie.d.berg@nasa.gov
NR 11
TC 2
Z9 2
U1 0
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD AUG
PY 2013
VL 60
IS 4
BP 2697
EP 2703
DI 10.1109/TNS.2013.2273938
PN 1
PG 7
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA 205NJ
UT WOS:000323450700047
ER
PT J
AU Tokay, A
Petersen, WA
Gatlin, P
Wingo, M
AF Tokay, Ali
Petersen, Walter A.
Gatlin, Patrick
Wingo, Matthew
TI Comparison of Raindrop Size Distribution Measurements by Collocated
Disdrometers
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
DE In situ atmospheric observations
ID TRMM PRECIPITATION RADAR; 2-DIMENSIONAL VIDEO DISDROMETER; SMALL-SCALE
VARIABILITY; DROP-SIZE; POLARIMETRIC RADAR; INSTRUMENTAL UNCERTAINTIES;
DISTRIBUTION MODEL; CONVECTIVE CLOUDS; DUAL-WAVELENGTH; RAINFALL
AB An impact-type Joss-Waldvogel disdrometer (JWD), a two-dimensional video disdrometer (2DVD), and a laser optical OTT Particle Size and Velocity (PARSIVEL) disdrometer (PD) were used to measure the raindrop size distribution (DSD) over a 6-month period in Huntsville, Alabama. Comparisons indicate event rain totals for all three disdrometers that were in reasonable agreement with a reference rain gauge. In a relative sense, hourly composite DSDs revealed that the JWD was more sensitive to small drops (<1 mm), while the PD appeared to severely underestimate small drops less than 0.76 mm in diameter. The JWD and 2DVD measured comparable number concentrations of midsize drops (1-3 mm) and large drops (3-5 mm), while the PD tended to measure relatively higher drop concentrations at sizes larger than 2.44 mm in diameter. This concentration disparity tended to occur when hourly rain rates and drop counts exceeded 2.5 mm h(-1) and 400 min(-1), respectively. Based on interactions with the PD manufacturer, the partially inhomogeneous laser beam is considered the cause of the PD drop count overestimation. PD drop fall speeds followed the expected terminal fall speed relationship quite well, while the 2DVD occasionally measured slower drops for diameters larger than 2.4 mm, coinciding with events where wind speeds were greater than 4 m s(-1). The underestimation of small drops by the PD had a pronounced effect on the intercept and shape of parameters of gamma-fitted DSDs, while the overestimation of midsize and larger drops resulted in higher mean values for PD integral rain parameters.
C1 [Tokay, Ali] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Petersen, Walter A.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Gatlin, Patrick] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Wingo, Matthew] Univ Alabama, Ctr Earth Syst Sci, Natl Space Sci & Technol Ctr, Huntsville, AL 35899 USA.
RP Tokay, A (reprint author), NASA, Goddard Space Flight Ctr, Code 612-0, Greenbelt, MD 20771 USA.
EM ali.tokay-1@nasa.gov
RI Measurement, Global/C-4698-2015;
OI Gatlin, Patrick/0000-0001-9345-1457
FU NASA's Global Precipitation Measurement mission of NASA Goddard Space
Flight Center; NASA's Precipitation Measurement Mission [NNX07AF45G,
NNX10AJ12G]
FX Feedback from the manufacturers of Joss-Waldvogel, OTT PARSIVEL, and the
two-dimensional video disdrometers are greatly appreciated.
Acknowledgements extended to the three anonymous reviewers for their
constructive comments. This study was funded under NASA's Global
Precipitation Measurement mission via Arthur Hou (GPM Project Scientist)
and Mathew Schwaller (GPM Ground Validation Project Manager) of NASA
Goddard Space Flight Center, and NASA's Precipitation Measurement
Mission (PMM) Grants NNX07AF45G and NNX10AJ12G, managed by Ramesh Kakar
of NASA Headquarters, Program Scientist.
NR 53
TC 44
Z9 45
U1 2
U2 28
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD AUG
PY 2013
VL 30
IS 8
BP 1672
EP 1690
DI 10.1175/JTECH-D-12-00163.1
PG 19
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 207XM
UT WOS:000323638000006
ER
PT J
AU Ilyushin, VV
Endres, CP
Lewen, F
Schlemmer, S
Drouin, BJ
AF Ilyushin, Vadim V.
Endres, Christian P.
Lewen, Frank
Schlemmer, Stephan
Drouin, Brian J.
TI Submillimeter wave spectrum of acetic acid
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Acetic acid; Submillimeter wave spectrum; Methyl top internal rotation;
Rho axis method
ID EXCITED TORSIONAL STATES; HOT MOLECULAR CORES; INTERNAL-ROTATION;
MILLIMETER-WAVE; MICROWAVE-SPECTRUM; COLOGNE DATABASE; METHYL CARBAMATE;
SPECTROSCOPY; METHANOL; CH3COOH
AB We present a new global study of the submillimeter wave spectrum of the lowest three torsional states of acetic acid (CH3COOH). New measurements involving torsion-rotation transitions with J up to 79 and K-a up to 44 have been carried out between 230 and 845 GHz using the submillimeter wave spectrometers in University of Cologne and Jet Propulsion Laboratory. The new data were combined with previously published measurements and fitted using the rho-axis-method torsion-rotation Hamiltonian. The final fit used 93 parameters to give an overall weighted root-mean-square deviation of 0.85 for a dataset consisting of 7543, 6087, and 5171 transitions belonging, respectively, to the ground, first, and second excited torsional states and 1888 Delta v(t) not equal 0 transitions. This investigation presents more than a twofold expansion both in the J quantum number and frequency range coverage of the acetic acid spectrum. Numerous inter-torsional interactions have been observed. Furthermore, this is the highest] value ever treated with the rho-axis-method and provides a good test case for the theoretical model in use. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Ilyushin, Vadim V.] Inst Radio Astron NASU, UA-61002 Kharkov, Ukraine.
[Endres, Christian P.; Lewen, Frank; Schlemmer, Stephan] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
[Drouin, Brian J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ilyushin, VV (reprint author), Inst Radio Astron NASU, Chervonopraporna 4, UA-61002 Kharkov, Ukraine.
EM ilyushin@rian.kharkov.ua
RI Schlemmer, Stephan/E-2903-2015
OI Schlemmer, Stephan/0000-0002-1421-7281
FU DAAD foundation; National Aeronautics and Space Administration
FX Vadim Ilyushin acknowledges financial support from the DAAD foundation
which made possible his stay in Cologne laboratory in 2008. Portions of
this paper present research carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 45
TC 6
Z9 6
U1 3
U2 16
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD AUG
PY 2013
VL 290
BP 31
EP 41
DI 10.1016/j.jms.2013.06.005
PG 11
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 207UB
UT WOS:000323629000006
ER
PT J
AU Pappalardo, RT
Vance, S
Bagenal, F
Bills, BG
Blaney, DL
Blankenship, DD
Brinckerhoff, WB
Connerney, JEP
Hand, KP
Hoehler, TM
Leisner, JS
Kurth, WS
McGrath, MA
Mellon, MT
Moore, JM
Patterson, GW
Prockter, LM
Senske, DA
Schmidt, BE
Shock, EL
Smith, DE
Soderlund, KM
AF Pappalardo, R. T.
Vance, S.
Bagenal, F.
Bills, B. G.
Blaney, D. L.
Blankenship, D. D.
Brinckerhoff, W. B.
Connerney, J. E. P.
Hand, K. P.
Hoehler, T. M.
Leisner, J. S.
Kurth, W. S.
McGrath, M. A.
Mellon, M. T.
Moore, J. M.
Patterson, G. W.
Prockter, L. M.
Senske, D. A.
Schmidt, B. E.
Shock, E. L.
Smith, D. E.
Soderlund, K. M.
TI Science Potential from a Europa Lander
SO ASTROBIOLOGY
LA English
DT Article
DE Mission; Planetary science; Ice; Europa; Icy moon
ID ICY GALILEAN SATELLITES; INFRARED MAPPING SPECTROMETER; HYDRATED SALT
MINERALS; TAGISH LAKE METEORITE; SUBSURFACE OCEAN; WATER-ICE;
SULFURIC-ACID; HYDROTHERMAL SYSTEMS; ENERGY-REQUIREMENTS; GEOLOGICAL
EVIDENCE
AB The prospect of a future soft landing on the surface of Europa is enticing, as it would create science opportunities that could not be achieved through flyby or orbital remote sensing, with direct relevance to Europa's potential habitability. Here, we summarize the science of a Europa lander concept, as developed by our NASA-commissioned Science Definition Team. The science concept concentrates on observations that can best be achieved by in situ examination of Europa from its surface. We discuss the suggested science objectives and investigations for a Europa lander mission, along with a model planning payload of instruments that could address these objectives. The highest priority is active sampling of Europa's non-ice material from at least two different depths (0.5-2 cm and 5-10 cm) to understand its detailed composition and chemistry and the specific nature of salts, any organic materials, and other contaminants. A secondary focus is geophysical prospecting of Europa, through seismology and magnetometry, to probe the satellite's ice shell and ocean. Finally, the surface geology can be characterized in situ at a human scale. A Europa lander could take advantage of the complex radiation environment of the satellite, landing where modeling suggests that radiation is about an order of magnitude less intense than in other regions. However, to choose a landing site that is safe and would yield the maximum science return, thorough reconnaissance of Europa would be required prior to selecting a scientifically optimized landing site.
C1 [Pappalardo, R. T.; Vance, S.; Bills, B. G.; Blaney, D. L.; Hand, K. P.] CALTECH, Jet Prop Lab, Planetary Sci Sect, Pasadena, CA 91109 USA.
[Bagenal, F.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO USA.
[Blankenship, D. D.; Schmidt, B. E.; Soderlund, K. M.] Univ Texas Austin, Inst Geophys, Austin, TX USA.
[Brinckerhoff, W. B.; Connerney, J. E. P.] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Hoehler, T. M.; Moore, J. M.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Leisner, J. S.; Kurth, W. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[McGrath, M. A.] Marshall Space Flight Ctr, Sci & Technol Off, Huntsville, AL USA.
[Mellon, M. T.] SW Res Inst, Planetary Sci Directorate, Boulder, CO USA.
[Patterson, G. W.; Prockter, L. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Senske, D. A.] CALTECH, Jet Prop Lab, Sci Res & Anal Program Off, Pasadena, CA 91109 USA.
[Shock, E. L.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Smith, D. E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA.
RP Pappalardo, RT (reprint author), CALTECH, Jet Prop Lab, Planetary Sci Sect, 4800 Oak Grove Dr,Mail Stop 321-560, Pasadena, CA 91109 USA.
EM robert.pappalardo@jpl.nasa.gov
RI Patterson, Gerald/E-7699-2015; Mellon, Michael/C-3456-2016;
OI Schmidt, Britney/0000-0001-7376-8510; Kurth, William/0000-0002-5471-6202
NR 188
TC 16
Z9 16
U1 5
U2 68
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD AUG
PY 2013
VL 13
IS 8
BP 740
EP 773
DI 10.1089/ast.2013.1003
PG 34
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 202IG
UT WOS:000323206900005
PM 23924246
ER
PT J
AU Brown, ME
Escobar, V
Moran, S
Entekhabi, D
O'Neill, PE
Njoku, EG
Doorn, B
Entin, JK
AF Brown, Molly E.
Escobar, Vanessa
Moran, Susan
Entekhabi, Dara
O'Neill, Peggy E.
Njoku, Eni G.
Doorn, Brad
Entin, Jared K.
TI NASA's Soil Moisture Active Passive (SMAP) Mission and Opportunities for
Applications Users
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
C1 [Brown, Molly E.; O'Neill, Peggy E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Escobar, Vanessa] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA.
[Moran, Susan] USDA ARS, Southwest Watershed Res Ctr, Tucson, AZ USA.
[Entekhabi, Dara] MIT, Cambridge, MA 02139 USA.
[Njoku, Eni G.] CALTECH, NASA, Jet Prop Lab, La Canada Flintridge, CA USA.
[Doorn, Brad; Entin, Jared K.] NASA Headquarters, Washington, DC USA.
RP Brown, ME (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
EM molly.brown@nasa.gov
RI Brown, Molly/M-5146-2013; Brown, Molly/E-2724-2010
OI Brown, Molly/0000-0001-7384-3314; Brown, Molly/0000-0001-7384-3314
NR 1
TC 13
Z9 13
U1 1
U2 28
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD AUG
PY 2013
VL 94
IS 8
BP 1125
EP 1128
DI 10.1175/BAMS-D-11-00049.1
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 205YZ
UT WOS:000323482200004
ER
PT J
AU Straneo, F
Heimbach, P
Sergienko, O
Hamilton, G
Catania, G
Griffies, S
Hallberg, R
Jenkins, A
Joughin, I
Motyka, R
Pfeffer, WT
Price, SF
Rignot, E
Scambos, T
Truffer, M
Vieli, A
AF Straneo, Fiammetta
Heimbach, Patrick
Sergienko, Olga
Hamilton, Gordon
Catania, Ginny
Griffies, Stephen
Hallberg, Robert
Jenkins, Adrian
Joughin, Ian
Motyka, Roman
Pfeffer, W. Tad
Price, Stephen F.
Rignot, Eric
Scambos, Ted
Truffer, Martin
Vieli, Andreas
TI Challenges to Understanding the Dynamic Response of Greenland's Marine
Terminating Glaciers to Oceanic and Atmospheric Forcing
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID SEA-LEVEL RISE; FULL STOKES MODEL; ICE-SHEET; JAKOBSHAVN ISBRAE; WEST
GREENLAND; OUTLET GLACIERS; EAST GREENLAND; THERMOHALINE CIRCULATION;
TIDEWATER GLACIERS; NORTH-ATLANTIC
AB The recent retreat and speedup of outlet glaciers, as well as enhanced surface melting around the ice sheet margin, have increased Greenland's contribution to sea level rise to 0.6 +/- 0.1 mm yr(-1) and its discharge of freshwater into the North Atlantic. The widespread, near-synchronous glacier retreat, and its coincidence with a period of oceanic and atmospheric warming, suggests a common climate driver. Evidence points to the marine margins of these glaciers as the region from which changes propagated inland. Yet, the forcings and mechanisms behind these dynamic responses are poorly understood and are either missing or crudely parameterized in climate and ice sheet models. Resulting projected sea level rise contributions from Greenland by 2100 remain highly uncertain. This paper summarizes the current state of knowledge and highlights key physical aspects of Greenland's coupled ice sheet-ocean-atmosphere system. Three research thrusts are identified to yield fundamental insights into ice sheet, ocean, sea ice, and atmosphere interactions, their role in Earth's climate system, and probable trajectories of future changes: 1) focused process studies addressing critical glacier, ocean, atmosphere, and coupled dynamics; 2) sustained observations at key sites; and 3) inclusion of relevant dynamics in Earth system models. Understanding the dynamic response of Greenland's glaciers to climate forcing constitutes both a scientific and technological frontier, given the challenges of obtaining the appropriate measurements from the glaciers' marine termini and the complexity of the dynamics involved, including the coupling of the ocean, atmosphere, glacier, and sea ice systems. Interdisciplinary and international cooperation are crucial to making progress on this novel and complex problem.
C1 [Straneo, Fiammetta] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Heimbach, Patrick] MIT, Cambridge, MA 02139 USA.
[Sergienko, Olga] Princeton Univ, Princeton, NJ 08544 USA.
[Sergienko, Olga; Griffies, Stephen; Hallberg, Robert] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Hamilton, Gordon] Univ Maine, Orono, ME USA.
[Catania, Ginny] Univ Texas Austin, Austin, TX 78712 USA.
[Jenkins, Adrian] British Antarctic Survey, Cambridge CB3 0ET, England.
[Joughin, Ian] Univ Washington, Seattle, WA 98195 USA.
[Motyka, Roman; Truffer, Martin] Univ Alaska Fairbanks, Fairbanks, AK USA.
[Pfeffer, W. Tad] Univ Colorado, Boulder, CO 80309 USA.
[Price, Stephen F.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Rignot, Eric] Univ Calif Irvine, Irvine, CA USA.
[Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Scambos, Ted] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA.
[Vieli, Andreas] Univ Durham, Durham, England.
RP Straneo, F (reprint author), Woods Hole Oceanog Inst, Mail Stop 21,266 Woods Hole Rd, Woods Hole, MA 02543 USA.
EM fstraneo@whoi.edu
RI Catania, Ginny/B-9787-2008; Heimbach, Patrick/K-3530-2013; Joughin,
Ian/A-2998-2008; Price, Stephen /E-1568-2013; Rignot, Eric/A-4560-2014;
OI Heimbach, Patrick/0000-0003-3925-6161; Joughin, Ian/0000-0001-6229-679X;
Price, Stephen /0000-0001-6878-2553; Rignot, Eric/0000-0002-3366-0481;
Vieli, Andreas/0000-0002-2870-5921; Straneo,
Fiammetta/0000-0002-1735-2366
FU Norwegian Centre for International Cooperation in Education (SiU)
FX This is a contribution to the activity of the U.S. CLIVAR Working Group
on Greenland Ice Sheet-Ocean Interactions (GRISO). Mike Patterson is
thanked for his engagement and guidance. The idea for establishment of
such a working group originated during the Advanced Climate Dynamics
Course (ACDC) 2010 on Ice Sheet-Ocean Interactions at the MIT-Fablab in
Lyngen, Norway (see
http://onlinelibrary.wiley.com/doi/10.1029/2010EO450006/abstract), with
the Norwegian Centre for International Cooperation in Education (SiU) as
its main sponsor. We thank three anonymous reviewers for their comments.
NR 97
TC 51
Z9 51
U1 0
U2 80
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 AUG
PY 2013
VL 94
IS 8
BP 1131
EP 1144
DI 10.1175/BAMS-D-12-00100.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 205YZ
UT WOS:000323482200005
ER
PT J
AU Ralph, FM
Intrieri, J
Andra, D
Atlas, R
Boukabara, S
Bright, D
Davidson, P
Entwistle, B
Gaynor, J
Goodman, S
Jiing, JG
Harless, A
Huang, J
Jedlovec, G
Kain, J
Koch, S
Kuo, B
Levit, J
Murillo, S
Riishojgaard, LP
Schneider, T
Schneider, R
Smith, T
Weiss, S
AF Ralph, F. Martin
Intrieri, Janet
Andra, David
Atlas, Robert
Boukabara, Sid
Bright, David
Davidson, Paula
Entwistle, Bruce
Gaynor, John
Goodman, Steve
Jiing, Jiann-Gwo
Harless, Amy
Huang, Jin
Jedlovec, Gary
Kain, John
Koch, Steven
Kuo, Bill
Levit, Jason
Murillo, Shirley
Riishojgaard, Lars Peter
Schneider, Timothy
Schneider, Russell
Smith, Travis
Weiss, Steven
TI The Emergence of Weather-Related Test Beds Linking Research and
Forecasting Operations
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID GOES-R; PRECIPITATION FORECASTS; DATA ASSIMILATION; SPRING PROGRAM; WRF
MODEL; PREDICTION; INFORMATION; SURFACE; INITIALIZATION; COLLABORATION
AB Test beds have emerged as a critical mechanism linking weather research with forecasting operations. The U.S. Weather Research Program (USWRP) was formed in the 1990s to help identify key gaps in research related to major weather prediction problems and the role of observations and numerical models. This planning effort ultimately revealed the need for greater capacity and new approaches to improve the connectivity between the research and forecasting enterprise. Out of this developed the seeds for what is now termed test beds. While many individual projects, and even more broadly the NOAA/National Weather Service (NWS) Modernization, were successful in advancing weather prediction services, it was recognized that specific forecast problems warranted a more focused and elevated level of effort. The USWRP helped develop these concepts with science teams and provided seed funding for several of the test beds described. Based on the varying NOAA mission requirements for forecasting, differences in the organizational structure and methods used to provide those services, and differences in the state of the science related to those forecast challenges, test beds have taken on differing characteristics, strategies, and priorities. Current test bed efforts described have all emerged between 2000 and 2011 and focus on hurricanes (Joint Hurricane Testbed), precipitation (Hydrometeorology Testbed), satellite data assimilation (Joint Center for Satellite Data Assimilation), severe weather (Hazardous Weather Testbed), satellite data support for severe weather prediction (Short-Term Prediction Research and Transition Center), mesoscale modeling (Developmental Testbed Center), climate forecast products (Climate Testbed), testing and evaluation of satellite capabilities [Geostationary Operational Environmental Satellite-R Series (GOES-R) Proving Ground], aviation applications (Aviation Weather Testbed), and observing system experiments (OSSE Testbed).
C1 [Ralph, F. Martin; Intrieri, Janet] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Andra, David] NOAA, Natl Weather Serv, Norman, OK USA.
[Atlas, Robert; Murillo, Shirley] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA.
[Boukabara, Sid; Riishojgaard, Lars Peter] Joint Ctr Satellite Data Assimilat, Camp Springs, MD USA.
[Bright, David; Entwistle, Bruce; Harless, Amy; Levit, Jason] NOAA, Natl Weather Serv, Natl Centers Environm Predict, Kansas City, MO USA.
[Davidson, Paula] NOAA, Natl Weather Serv, Off Sci & Technol, Silver Spring, MD 20910 USA.
[Gaynor, John] NOAA, Off Policy Planning & Evaluat, Silver Spring, MD USA.
[Gaynor, John] NOAA, Natl Environm Satellite Data & Informat Serv, Greenbelt, MD USA.
[Goodman, Steve] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jiing, Jiann-Gwo] NOAA, Natl Hurricane Ctr, Miami Beach, FL USA.
[Huang, Jin] NOAA, Natl Weather Serv, Climate Predict Ctr, Camp Springs, MD USA.
[Jedlovec, Gary] NASA, Marshall Space Flight Ctr, Huntsville, AL USA.
[Kain, John; Koch, Steven; Smith, Travis] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA.
[Kain, John; Koch, Steven; Smith, Travis] Univ Oklahoma, Cooperat Inst Mesoscale Meteorol Studies, Norman, OK 73019 USA.
[Kuo, Bill] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Schneider, Timothy] NOAA, Natl Weather Serv, Off Hydrol Dev, Boulder, CO USA.
[Schneider, Russell; Weiss, Steven] NOAA, Natl Weather Serv, Storm Predict Ctr, Norman, OK USA.
RP Ralph, FM (reprint author), NOAA, Earth Syst Res Lab, R E PSD, 325 Broadway, Boulder, CO 80305 USA.
EM marty.ralph@noaa.gov
RI Atlas, Robert/A-5963-2011; Boukabara, Sid Ahmed/F-5577-2010; Murillo,
Shirley/C-3259-2014; Intrieri, Janet/D-5608-2015; Schneider,
Timothy/D-2832-2015
OI Atlas, Robert/0000-0002-0706-3560; Boukabara, Sid
Ahmed/0000-0002-1857-3806; Murillo, Shirley/0000-0002-2075-8682;
FU U.S. Weather Research Program in NOAA/OAR's Office of Weather and Air
Quality; NSSL; NWS/SPC; NWS/Norman WFO; NOAA/OAR under the
NOAA-University of Oklahoma, U.S. Department of Commerce
[NA08OAR4320904]; NOAA; U.S. Air Force; NSF; NCAR; NCEP; NOAA Climate
Program Office; Earth Science Division at NASA headquarters; NOAA GOES-R
Program Science Office
FX The U.S. Weather Research Program in NOAA/OAR's Office of Weather and
Air Quality provides full support for JHT, partial support for HMT and
DTC, and seed funding for the OSSE Testbed. The HWT is jointly funded
and managed by NSSL, NWS/SPC, and NWS/Norman WFO, with NSSL providing
funding for the majority of the infrastructure. Funding is also provided
by NOAA/OAR under the NOAA-University of Oklahoma Cooperative Agreement
NA08OAR4320904, U.S. Department of Commerce. The DTC is jointly
sponsored by the NOAA, U.S. Air Force, NSF, and NCAR. NCEP and the NOAA
Climate Program Office jointly support the CTB. SPoRT is funded by the
Earth Science Division at NASA headquarters and the NOAA GOES-R Program
Science Office. The NOAA GOES-R Program Science Office supports the
GOES-R Proving Ground.
NR 57
TC 20
Z9 25
U1 2
U2 21
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 AUG
PY 2013
VL 94
IS 8
BP 1187
EP 1211
DI 10.1175/BAMS-D-12-00080.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 205YZ
UT WOS:000323482200008
ER
PT J
AU Bosilovich, MG
Chaudhuri, AH
Rixen, M
AF Bosilovich, Michael G.
Chaudhuri, Ayan H.
Rixen, Michel
TI Earth System Reanalysis: Progress, Challenges, and Opportunities
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
C1 [Bosilovich, Michael G.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Chaudhuri, Ayan H.] Atmospher & Environm Res Inc, Lexington, MA USA.
[Rixen, Michel] World Climate Res Programme, Geneva, Switzerland.
RP Bosilovich, MG (reprint author), NASA, Goddard Space Flight Ctr, Div Earth Sci, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA.
EM michael.bosilovich@nasa.gov
RI Bosilovich, Michael/F-8175-2012
FU NASA; NOAA; National Science Foundation; U.S. Department of Energy;
European Space Agency; European Geosciences Union
FX Sponsorship from NASA, NOAA, the National Science Foundation, the U.S.
Department of Energy, the European Space Agency, and the European
Geosciences Union greatly contributed to the success of this conference
and is deeply acknowledged.
NR 0
TC 2
Z9 2
U1 0
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD AUG
PY 2013
VL 94
IS 8
BP ES110
EP ES113
DI 10.1175/BAMS-D-12-00191.1
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 205YZ
UT WOS:000323482200002
ER
PT J
AU Shebalin, JV
AF Shebalin, John V.
TI Broken ergodicity in magnetohydrodynamic turbulence
SO GEOPHYSICAL AND ASTROPHYSICAL FLUID DYNAMICS
LA English
DT Article
DE Magnetohydrodynamics; Turbulence; Statistical mechanics; Dynamo theory
ID ROTATING SPHERICAL-SHELL; MAGNETIC DYNAMO ACTION; ISOTROPIC TURBULENCE;
COMPRESSIBLE CONVECTION; NUMERICAL-SIMULATION; RELAXATION; FIELDS;
FLUCTUATIONS; GENERATION; FLOWS
AB Turbulent magnetofluids appear in various geophysical and astrophysical contexts, in phenomena associated with planets, stars, galaxies and the universe itself. In many cases, large-scale magnetic fields are observed, though a better knowledge of magnetofluid turbulence is needed to more fully understand the dynamo processes that produce them. One approach is to develop the statistical mechanics of ideal (i.e. non-dissipative), incompressible, homogeneous magnetohydrodynamic (MHD) turbulence, known as absolute equilibrium ensemble theory, as far as possible by studying model systems with the goal of finding those aspects that survive the introduction of viscosity and resistivity. Here, we review the progress that has been made in this direction. We examine both three-dimensional (3-D) and two-dimensional (2-D) model systems based on discrete Fourier representations. The basic equations are those of incompressible MHD and may include the effects of rotation and/or a mean magnetic field B-o. Statistical predictions are that Fourier coefficients of the velocity and magnetic field are zero-mean random variables. However, this is not the case, in general, for we observe non-ergodic behavior in very long time computer simulations of ideal turbulence: low wavenumber Fourier modes that have relatively large means and small standard deviations, i.e. coherent structure. In particular, ergodicity appears strongly broken when B-o= 0 and weakly broken when B-o not equal 0. Broken ergodicity in MHD turbulence is explained by an eigenanalysis of modal covariance matrices. This produces a set of modal eigenvalues inversely proportional to the expected energy of their associated eigenvariables. A large disparity in eigenvalues within the same mode (identified by wavevector k) can occur at low values of wavenumber k=vertical bar k vertical bar, especially when B-o = 0. This disparity breaks the ergodicity of eigenvariables with smallest eigenvalues (largest energies). This leads to coherent structure in models of ideal homogeneous MHD turbulence, which can occur at lowest values of wavenumber k for 3-D cases, and at either lowest or highest k for ideal 2-D magnetofluids. These ideal results appear relevant for unforced, decaying MHD turbulence, so that broken ergodicity effects in MHD turbulence survive dissipation. In comparison, we will also examine ideal hydrodynamic (HD) turbulence, which, in the 3-D case, will be seen to differ fundamentally from ideal MHD turbulence in that coherent structure due to broken ergodicity can only occur at maximum k in numerical simulations. However, a nonzero viscosity eliminates this ideal 3-D HD structure, so that unforced, decaying 3-D HD turbulence is expected to be ergodic. In summary, broken ergodicity in MHD turbulence leads to energetic, large-scale, quasistationary magnetic fields (coherent structures) in numerical models of bounded, turbulent magnetofluids. Thus, broken ergodicity provides a large-scale dynamo mechanism within computer models of homogeneous MHD turbulence. These results may help us to better understand the origin of global magnetic fields in astrophysical and geophysical objects.
C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Shebalin, JV (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code KR, Houston, TX 77058 USA.
EM john.v.shebalin@nasa.gov
NR 69
TC 4
Z9 4
U1 0
U2 4
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 0309-1929
EI 1029-0419
J9 GEOPHYS ASTRO FLUID
JI Geophys. Astrophys. Fluid Dyn.
PD AUG 1
PY 2013
VL 107
IS 4
SI SI
BP 411
EP 466
DI 10.1080/03091929.2011.589385
PG 56
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Mechanics
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Mechanics
GA 196IG
UT WOS:000322766900002
ER
PT J
AU Yamada, TJ
Kanae, S
Oki, T
Koster, RD
AF Yamada, Tomohito J.
Kanae, Shinjiro
Oki, Taikan
Koster, Randal D.
TI Seasonal variation of land-atmosphere coupling strength over the West
African monsoon region in an atmospheric general circulation model
SO HYDROLOGICAL SCIENCES JOURNAL-JOURNAL DES SCIENCES HYDROLOGIQUES
LA English
DT Article
DE land-atmosphere interactions; coupling strength; West African monsoon;
soil moisture; evapotranspiration; AGCM
ID SURFACE TEMPERATURE ANOMALIES; SOIL-MOISTURE MEMORY; PART I;
PRECIPITATION; PREDICTABILITY; CLIMATE; PREDICTION; WETNESS; IMPACT;
GLACE
AB The seasonal variation of land-atmosphere coupling strength has been examined using an extended series of atmospheric general circulation model (AGCM) simulations. In the Western Sahel of Africa, strong coupling strength for precipitation is found in April and May, just prior to and at the beginning of the monsoon season. At this time, heat and water fluxes from the surface are strongly controlled by land conditions, and the unstable conditions in the lower level of the troposphere, as induced by local land state, allow the surface fluxes to influence the variability of convective precipitationand thus the timing of monsoon onset.
C1 [Yamada, Tomohito J.] Hokkaido Univ, Fac Engn, Sapporo, Hokkaido 060, Japan.
[Kanae, Shinjiro] Tokyo Inst Technol, Dept Mech & Environm Informat, Tokyo 1528552, Japan.
[Oki, Taikan] Univ Tokyo, Inst Ind Sci, Tokyo 1538505, Japan.
[Koster, Randal D.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Yamada, TJ (reprint author), Kita 13 Nishi 8,Kita Ku, Sapporo, Hokkaido 0608628, Japan.
EM tomohito@eng.hokudai.ac.jp
RI Koster, Randal/F-5881-2012; Oki, Taikan/E-5778-2010; Kanae,
Shinjiro/E-5606-2010; PMM, JAXA/K-8537-2016
OI Koster, Randal/0000-0001-6418-6383; Oki, Taikan/0000-0003-4067-4678;
Kanae, Shinjiro/0000-0002-3176-4957;
FU MEXT SOUSEI programme (Theme C-i-C); Research Programme on Climate
Change Adaptation (RECCA/MEXT); Science Technology Research Partnership
for Sustainable Development (IMPAC-T, JST-JICA); Core Research for
Evolutional Science and Technology programme (CREST/JST); Japan
Aerospace Exploration Agency (JAXA) PMM Mission
FX This work was supported by the MEXT SOUSEI programme (Theme C-i-C), the
Research Programme on Climate Change Adaptation (RECCA/MEXT), the
Science Technology Research Partnership for Sustainable Development
(IMPAC-T, JST-JICA), the Core Research for Evolutional Science and
Technology programme (CREST/JST) and the Japan Aerospace Exploration
Agency (JAXA) PMM Mission. All computational resources were provided by
the National Institute for Environmental Studies.
NR 38
TC 5
Z9 5
U1 0
U2 15
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0262-6667
J9 HYDROLOG SCI J
JI Hydrol. Sci. J.-J. Sci. Hydrol.
PD AUG 1
PY 2013
VL 58
IS 6
BP 1276
EP 1286
DI 10.1080/02626667.2013.814914
PG 11
WC Water Resources
SC Water Resources
GA 202TJ
UT WOS:000323242200004
ER
PT J
AU Li, SR
De Geronimo, G
Chen, W
D'Anadragora, A
Fried, J
Li, Z
Pinelli, DA
Smith, GC
Gaskin, JA
Ramsey, BD
AF Li, Shaorui
De Geronimo, Gianluigi
Chen, Wei
D'Anadragora, Alessio
Fried, Jack
Li, Zheng
Pinelli, Donald A.
Smith, Graham C.
Gaskin, Jessica A.
Ramsey, Brian D.
TI A Low-Power, Radiation-Resistant ASIC for SDD-Based X-Ray Spectrometers
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE ASIC; radiation-resistant; SDD; x-ray spectrometer.
ID COMMERCIAL CMOS TECHNOLOGIES; ISOLATION OXIDES; DEGRADATION
AB We present an Application Specific Integrated Circuit (ASIC) for high resolution X-ray spectrometers (XRS) in radiation harsh environment (such as Jovian system). The ASIC was designed to read out signals from low resistivity pixelated Silicon-Drift-Detectors (SDD) to ensure radiation hardness. The readout is done by wire-bonding the anodes to the inputs of the ASIC. The ASIC dissipates 32 mW and provides 16 channels of low-noise charge amplification, high-order shaping with baseline stabilization, discrimination, pile-up rejection, and peak detection with analog memory. The readout is sparse and based on a custom low-power tri-stable low-voltage differential signaling digital interface. A unit of 64 SDD pixels, read out by four ASICs, covers an area of 12.8 cm(2), and dissipates less than 20 mW/cm(2). The ASICs were powered on and irradiated using a beam line with 203 MeV protons, to total doses ranging from 0.25 Mrad to 12 Mrad. Performance degradation due to radiation-induced leakage current was observed to peak around 2 Mrad dose. Critical contributors to the degradation were identified through simulation and measurements, and corresponding circuitry was thus modified to address the issues. Measurements on the radiation-resistant design have shown excellent radiation resistance at total doses ranging from 1 to 8 Mrad.
C1 [Li, Shaorui; De Geronimo, Gianluigi; Chen, Wei; D'Anadragora, Alessio; Fried, Jack; Li, Zheng; Pinelli, Donald A.; Smith, Graham C.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Gaskin, Jessica A.; Ramsey, Brian D.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Li, SR (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA.
EM shaoruili@bnl.gov
FU U.S. Department of Energy [DE-AC02-98CH10886]; NASA Research
Opportunities in Space and Earth Science, Planetary Instrument
Definition and Development Program
FX This work was supported in part by the U.S. Department of Energy under
Contract DE-AC02-98CH10886, and in part by the NASA Research
Opportunities in Space and Earth Science, Planetary Instrument
Definition and Development Program.
NR 13
TC 0
Z9 0
U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD AUG
PY 2013
VL 60
IS 4
BP 3057
EP 3062
DI 10.1109/TNS.2013.2268980
PN 2
PG 6
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA 205NT
UT WOS:000323451800028
ER
PT J
AU Howell, SB
Rector, TA
Walter, D
AF Howell, Steve B.
Rector, Travis A.
Walter, Donald
TI Optical Spectroscopy at Deep Light Minimum of R Coronae Borealis
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE Stars
ID IRON CURTAIN; XX-OPH; STARS; DECLINE; HELIUM; DUST
AB We present optical spectroscopy late in a deep minimum for the quintessential hydrogen-deficient carbon star R Coronae Borealis. Starting 3.5 years into the current deep and long minimum, we have secured observations that reveal some of the oddest optical spectra ever obtained for any astronomical object. Helium emission lines from triplet transitions, strong Ca II H and K emission, and forbidden lines of oxygen and nitrogen are the only spectral features observed. The spectra can be interpreted as coming from a chromospheric-like region lying above a carbon shell ejection front combined with a large-scale nebular-like region surrounding the star.
"The variable star R Coronae Borealis is a jewel worthy of a place in any crown. It is one of the most interesting and most peculiar of all variables, and is often called the ideal irregular variable. Its times of minimum are distributed at random, according to the laws of pure chanceMargaret"- Mayall (1962)
C1 [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rector, Travis A.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Walter, Donald] South Carolina State Univ, Dept Biol & Phys Sci, Orangeburg, SC 29115 USA.
RP Howell, SB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
NR 34
TC 2
Z9 2
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD AUG
PY 2013
VL 125
IS 930
BP 879
EP 888
DI 10.1086/672163
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205FR
UT WOS:000323428900001
ER
PT J
AU Bryson, ST
Jenkins, JM
Gilliland, RL
Twicken, JD
Clarke, B
Rowe, J
Caldwell, D
Batalha, N
Mullally, F
Haas, MR
Tenenbaum, P
AF Bryson, Stephen T.
Jenkins, Jon M.
Gilliland, Ronald L.
Twicken, Joseph D.
Clarke, Bruce
Rowe, Jason
Caldwell, Douglas
Batalha, Natalie
Mullally, Fergal
Haas, Michael R.
Tenenbaum, Peter
TI Identification of Background False Positives from Kepler Data
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE Extrasolar Planets
ID PERFORMANCE
AB The Kepler Mission was launched on 2009 March 6 to perform a photometric survey of more than 100,000 dwarf stars to search for Earth-size planets with the transit technique. The reliability of the resulting planetary candidate list relies on the ability to identify and remove false positives. Major sources of astrophysical false positives are planetary transits and stellar eclipses on background stars. We describe several new techniques for the identification of background transit sources that are separated from their target stars, indicating an astrophysical false positive. These techniques use only Kepler photometric data. We describe the concepts and construction of these techniques in detail as well as their performance and relative merits.
C1 [Bryson, Stephen T.; Haas, Michael R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Jenkins, Jon M.; Twicken, Joseph D.; Clarke, Bruce; Rowe, Jason; Caldwell, Douglas; Mullally, Fergal; Tenenbaum, Peter] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
RP Bryson, ST (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM steve.bryson@nasa.gov
RI Caldwell, Douglas/L-7911-2014
OI Caldwell, Douglas/0000-0003-1963-9616
FU Kepler Science Operations Center and Science Office
FX We gratefully acknowledge the outstanding work of the entire Kepler team
that performs the data acquisition and analysis and delivers the
precision that makes the techniques described in this paper possible. We
particularly thank the Kepler Science Operations Center and Science
Office for their support and creativity while these techniques were
being developed. We thank Martin Still, Susan Thompson, and Jeff
Coughlin for valuable comments on early drafts of this paper. Finally,
we thank Bill Borucki, Ted Dunham, Dave Latham, Nick Gautier, and the
wider Kepler science community for constant support and encouragement.
NR 13
TC 51
Z9 51
U1 2
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD AUG
PY 2013
VL 125
IS 930
BP 889
EP 923
DI 10.1086/671767
PG 35
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205FR
UT WOS:000323428900002
ER
PT J
AU Guyon, O
Mennesson, B
Serabyn, E
Martin, S
AF Guyon, Olivier
Mennesson, Bertrand
Serabyn, Eugene
Martin, Stefan
TI Optimal Beam Combiner Design for Nulling Interferometers
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE Astronomical Instrumentation
ID EXTRASOLAR PLANETS; ARRAY CONFIGURATIONS; SEARCH; SPACE; LIFE;
CORONAGRAPHY; TELESCOPES; MISSION; FUTURE; FINDER
AB A scheme to optimally design a beam combiner is discussed for any predetermined fixed geometry nulling interferometer aimed at detection and characterization of exoplanets with multiple telescopes or a single telescope (aperture masking). We show that considerably higher order nulls can be achieved with 1D (one-dimensional) interferometer geometries than possible with 2D (two-dimensional) geometries with the same number of apertures. Any 1D interferometer with apertures can achieve a (N - 1)-order null, while the order of the deepest null for a random 2D aperture geometry interferometer is the order of the th term in the Taylor expansion of e(i)((x3+y2))around x = 0, y = 0 (2nd order null for N = 2, 3; 4th order null for N = 4, 5, 6 ). We also show that an optimal beam combiner for nulling interferometry relies on only 0 or pi phase shifts. Examples of nulling interferometer designs are shown to illustrate these findings.
C1 [Guyon, Olivier] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Guyon, Olivier] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Mennesson, Bertrand; Serabyn, Eugene; Martin, Stefan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Guyon, O (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
EM guyon@naoj.org
NR 28
TC 0
Z9 0
U1 0
U2 1
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 AUG
PY 2013
VL 125
IS 930
BP 951
EP 965
DI 10.1086/671816
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 205FR
UT WOS:000323428900005
ER
EF