= 317 +/- 21 km s(-1). Considering the weaker statistical correlation in the GC r(h) color and the GC r(h)-R-gal relations, the more significant GC size-dynamics relation appears to be astrophysically more relevant and hints at the dominant influence of the GC orbit distribution function on the evolution of GC structural parameters.
C1 [Puzia, Thomas H.] Pontificia Univ Catolica Chile, Natl Res Council Canada, Santiago 7820436, Chile.
[Puzia, Thomas H.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Paolillo, Maurizio] Univ Naples Federico II, Dept Phys Sci, I-80126 Naples, Italy.
[Paolillo, Maurizio] Ist Nazl Fis Nucl, Dept Phys Sci, Napoli Unit, I-80126 Naples, Italy.
[Paolillo, Maurizio] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy.
[Goudfrooij, Paul] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Maccarone, Thomas J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
[Fabbiano, Giuseppina] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Angelini, Lorella] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA.
RP Puzia, TH (reprint author), Pontificia Univ Catolica Chile, Natl Res Council Canada, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile.
EM tpuzia@astro.puc.cl
RI Paolillo, Maurizio/J-1733-2012
OI Paolillo, Maurizio/0000-0003-4210-7693
FU NASA [NAS5-26555]; FONDECYT [1121005]; BASAL Center for Astrophysics and
Associated Technologies [PFB-06]; National Research Council of Canada;
University of Napoli Federico II; Chandra X-ray Center (CXC)
[NAS8-03060]
FX Support for HST program GO- 10129 was provided by NASA through a grant
from the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Incorporated,
under NASA contract NAS5-26555. This research was supported by FONDECYT
Regular Project grant 1121005 and BASAL Center for Astrophysics and
Associated Technologies (PFB-06). T. H. P. is thankful for the
hospitality and support during his visits at the University of Napoli
Federico II, where parts of this work were completed; he also gratefully
acknowledges support in the form of a Plaskett Research Fellowship from
the National Research Council of Canada. M. P. acknowledges financial
support from the FARO 2011 project of the University of Napoli Federico
II. This work was partially supported by the Chandra X-ray Center (CXC),
which is operated by the Smithsonian Astrophysical Observatory (SAO)
under NASA contract NAS8-03060. We are grateful to Anton Koekemoer and
Andy Fruchter for their technical support and useful discussions on the
MultiDrizzle code and to Chien Y. Peng for his help with the
implementation and testing of the modified GALFIT routine. We thank
TomRichtler and Ylva Schuberth for providing their radial velocity
measurements ahead of publication, as well as Luis Ho and Zhao-Yu Li for
kindly making available to us their latest NGC 1399 surface brightness
profile measurements from the Carnegie-Irvine Galaxy Survey, again prior
to publication. Avon Huxor has very kindly supplied M31 GC data prior to
publication. We are grateful to the referee, Bill Harris, for providing
a thoughtful and constructive report that helped improve the
presentation of the results. We thank Jeremy Webb, Mark Gieles, Andres
Jordan, Eric Peng, Chunyan Jiang, Stephen Zepf, and Arunav Kundu for
valuable discussions and providing data in electronic format. 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 NNX09AF08G and
by other grants and contracts. This research has made use of the
NASA/IPAC Infrared Science Archive, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. Figures
2 and 3 were created with the help of the ESA/ESO/NASA Photoshop FITS
Liberator. This research has made use of NASA's Astrophysics Data
System. Facility: HST(ACS)
NR 171
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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 MAY 10
PY 2014
VL 786
IS 2
AR 78
DI 10.1088/0004-637X/786/2/78
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH1MI
UT WOS:000335884500002
ER
PT J
AU Rivers, E
Markowitz, A
Rothschild, R
Bamba, A
Fukazawa, Y
Okajima, T
Reeves, J
Terashima, Y
Ueda, Y
AF Rivers, Elizabeth
Markowitz, Alex
Rothschild, Richard
Bamba, Aya
Fukazawa, Yasushi
Okajima, Takashi
Reeves, James
Terashima, Yuichi
Ueda, Yoshihiro
TI TRACKING THE COMPLEX ABSORPTION IN NGC 2110 WITH TWO SUZAKU OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 2110); X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; LINE GALAXY NGC-2110; X-RAY BINARIES;
BLACK-HOLE; XMM-NEWTON; INTERSTELLAR-MEDIUM; SEYFERT-GALAXIES; EMISSION;
SPECTROSCOPY; REFLECTION
AB We present spectral analysis of two Suzaku observations of the Seyfert 2 galaxy, NGC 2110. This source has been known to show complex, variable absorption which we study in depth by analyzing these two observations set 7 yr apart and by comparing them to previously analyzed observations with the XMM-Newton and Chandra observatories. We find that there is a relatively stable, full-covering absorber with a column density of similar to 3 x 10(22) cm(-2), with an additional patchy absorber that is likely variable in both column density and covering fraction over timescales of years, consistent with clouds in a patchy torus or in the broad line region. We model a soft emission line complex, likely arising from ionized plasma and consistent with previous studies. We find no evidence for reflection from an accretion disk in this source with contribution from neither relativistically broadened Fe K alpha line emission, nor from a Compton reflection hump.
C1 [Rivers, Elizabeth; Markowitz, Alex; Rothschild, Richard] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Rivers, Elizabeth] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Markowitz, Alex] Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany.
[Bamba, Aya] Aoyama Gakuin Univ, Dept Math & Phys, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan.
[Fukazawa, Yasushi] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Okajima, Takashi] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Reeves, James] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Terashima, Yuichi] Ehime Univ, Dept Phys, Matsuyama, Ehime 7908577, Japan.
[Ueda, Yoshihiro] Kyoto Univ, Dept Astron, Kyoto 6068502, Japan.
RP Rivers, E (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA.
EM erivers@caltech.edu
RI XRAY, SUZAKU/A-1808-2009
FU NASA/GSFC; NASA/IPAC Extragalactic Database; [NNX13AF33G]
FX This research has made use of data obtained from the Suzaku satellite, a
collaborative mission between the space agencies of Japan (JAXA) and the
USA (NASA). This work has made use of HEASARC online services, supported
by NASA/GSFC, and the NASA/IPAC Extragalactic Database, operated by
JPL/California Institute of Technology under contract with NASA. This
research was supported by Grant NNX13AF33G.
NR 42
TC 9
Z9 9
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2014
VL 786
IS 2
AR 126
DI 10.1088/0004-637X/786/2/126
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH1MI
UT WOS:000335884500050
ER
PT J
AU Tian, H
DeLuca, E
Reeves, KK
McKillop, S
De Pontieu, B
Martinez-Sykora, J
Carlsson, M
Hansteen, V
Kleint, L
Cheung, M
Golub, L
Saar, S
Testa, P
Weber, M
Lemen, J
Title, A
Boerner, P
Hurlburt, N
Tarbell, TD
Wuelser, JP
Kankelborg, C
Jaeggli, S
McIntosh, SW
AF Tian, H.
DeLuca, E.
Reeves, K. K.
McKillop, S.
De Pontieu, B.
Martinez-Sykora, J.
Carlsson, M.
Hansteen, V.
Kleint, L.
Cheung, M.
Golub, L.
Saar, S.
Testa, P.
Weber, M.
Lemen, J.
Title, A.
Boerner, P.
Hurlburt, N.
Tarbell, T. D.
Wuelser, J. P.
Kankelborg, C.
Jaeggli, S.
McIntosh, S. W.
TI HIGH-RESOLUTION OBSERVATIONS OF THE SHOCK WAVE BEHAVIOR FOR SUNSPOT
OSCILLATIONS WITH THE INTERFACE REGION IMAGING SPECTROGRAPH
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE line: profiles; Sun: chromosphere; Sun: oscillations; Sun: transition
region; waves
ID RUNNING PENUMBRAL WAVES; TRANSITION REGION; DYNAMIC FIBRILS;
SPECTROSCOPIC OBSERVATIONS; MAGNETOACOUSTIC SHOCKS; NUMERICAL
SIMULATIONS; PROPAGATING WAVES; ATOMIC DATABASE; UMBRAL FLASHES; CORONAL
LOOPS
AB We present the first results of sunspot oscillations from observations by the Interface Region Imaging Spectrograph. The strongly nonlinear oscillation is identified in both the slit-jaw images and the spectra of several emission lines formed in the transition region and chromosphere. We first apply a single Gaussian fit to the profiles of the Mg II 2796.35 angstrom, C II 1335.71 angstrom, and Si IV 1393.76 angstrom lines in the sunspot. The intensity change is similar to 30%. The Doppler shift oscillation reveals a saw tooth pattern with an amplitude of similar to 10 km s(-1) in Si IV. The Si IV oscillation lags those of C II and Mg II by similar to 6 and similar to 25 s, respectively. The line width suddenly increases as the Doppler shift changes from redshift to blueshift. However, we demonstrate that this increase is caused by the superposition of two emission components. We then perform detailed analysis of the line profiles at a few selected locations on the slit. The temporal evolution of the line core is dominated by the following behavior: a rapid excursion to the blue side, accompanied by an intensity increase, followed by a linear decrease of the velocity to the red side. The maximum intensity slightly lags the maximum blueshift in Si IV, whereas the intensity enhancement slightly precedes the maximum blueshift in Mg II. We find a positive correlation between the maximum velocity and deceleration, a result that is consistent with numerical simulations of upward propagating magnetoacoustic shock waves.
C1 [Tian, H.; DeLuca, E.; Reeves, K. K.; McKillop, S.; Golub, L.; Saar, S.; Testa, P.; Weber, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[De Pontieu, B.; Martinez-Sykora, J.; Kleint, L.; Cheung, M.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Martinez-Sykora, J.; Kleint, L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Carlsson, M.; Hansteen, V.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway.
[Kleint, L.] NASA, Ames Res Ctr, Moffett Field, CA 94305 USA.
[Kankelborg, C.; Jaeggli, S.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
[McIntosh, S. W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
RP Tian, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM hui.tian@cfa.harvard.edu
RI Reeves, Katharine/P-9163-2014; DeLuca, Edward/L-7534-2013;
OI DeLuca, Edward/0000-0001-7416-2895; Carlsson, Mats/0000-0001-9218-3139
FU NASA [NNG09FA40C]; Lockheed Martin Independent Research Program;
European Research Council [291058]; LMSAL [8100002705]
FX IRIS is a NASA small explorer mission developed and operated by LMSAL
with mission operations executed at NASA Ames Research center and major
contributions to downlink communications funded by the Norwegian Space
Center (NSC, Norway) through an ESA PRODEX contract. This work is
supported by NASA under contract NNG09FA40C (IRIS) and the Lockheed
Martin Independent Research Program, the European Research Council grant
agreement No. 291058, and contract 8100002705 from LMSAL to SAO. H. T.
thanks Luc Rouppe van der Voort and Jorrit Leenaarts for useful
discussion.
NR 56
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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
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2014
VL 786
IS 2
AR 137
DI 10.1088/0004-637X/786/2/137
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH1MI
UT WOS:000335884500060
ER
PT J
AU Vinas, AF
Moya, PS
Araneda, JA
Maneva, YG
AF Vinas, Adolfo F.
Moya, Pablo S.
Araneda, Jaime A.
Maneva, Yana G.
TI RECONSTRUCTION OF A BROADBAND SPECTRUM OF ALFVENIC FLUCTUATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; methods: analytical; turbulence; waves
ID SOLAR-WIND TURBULENCE; MAGNETIC HELICITY; INTERPLANETARY SHOCKS; HYBRID
SIMULATIONS; CYCLOTRON WAVES; INSTABILITY; EVOLUTION; DECAY; ANGLE;
FIELD
AB Alfvenic fluctuations in the solar wind exhibit a high degree of velocities and magnetic field correlations consistent with Alfven waves propagating away and toward the Sun. Two remarkable properties of these fluctuations are the tendencies to have either positive or negative magnetic helicity (-1 <= sigma(m) <= + 1) associated with either left-or righttopological handedness of the fluctuations and to have a constant magnetic field magnitude. This paper provides, for the first time, a theoretical framework for reconstructing both the magnetic and velocity field fluctuations with a divergence-free magnetic field, with any specified power spectral index and normalized magnetic-and cross-helicity spectrum field fluctuations for any plasma species. The spectrum is constructed in the Fourier domain by imposing two conditions-a divergence-free magnetic field and the preservation of the sense of magnetic helicity in both spaces-as well as using Parseval's theorem for the conservation of energy between configuration and Fourier spaces. Applications to the one-dimensional spatial Alfvenic propagation are presented. The theoretical construction is in agreement with typical time series and power spectra properties observed in the solar wind. The theoretical ideas presented in this spectral reconstruction provide a foundation for more realistic simulations of plasma waves, solar wind turbulence, and the propagation of energetic particles in such fluctuating fields.
C1 [Vinas, Adolfo F.; Moya, Pablo S.; Maneva, Yana G.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Moya, Pablo S.; Maneva, Yana G.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Araneda, Jaime A.] Univ Concepcion, Fac Ciencias Fis & Matemat, Dept Fis, Concepcion, Chile.
RP Vinas, AF (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Mail Code 673, Greenbelt, MD 20771 USA.
EM adolfo.vinas@nasa.gov
RI Moya, Pablo/C-3163-2011; Araneda, Jaime/J-9245-2015;
OI Moya, Pablo/0000-0002-9161-0888; Maneva, Yana/0000-0002-2422-6050
FU NASA Wind/SWE program; Comision Nacional de Ciencia y Tecnologia
(CONICyT, Chile); NASA Wind program; FONDECYT [1110880]; CUA
post-doctoral program
FX We thank Dr. Robert Wicks for providing critical suggestions and
comments on this paper, and the NASA Wind/SWE program for the support of
this research. We also thank the Comision Nacional de Ciencia y
Tecnologia (CONICyT, Chile) for providing financial support for P.S.M.'s
postdoctoral fellowship. Y.M. thanks the NASA Wind and CUA post-doctoral
programs for their financial support. J.A.A. thanks FONDECYT (No.
1110880) for providing financial support.
NR 25
TC 3
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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 MAY 10
PY 2014
VL 786
IS 2
AR 86
DI 10.1088/0004-637X/786/2/86
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH1MI
UT WOS:000335884500010
ER
PT J
AU Yu, SS
Pearson, JC
AF Yu, Shanshan
Pearson, John C.
TI TERAHERTZ MEASUREMENTS OF THE HOT HYDRONIUM ION WITH AN EXTENDED
NEGATIVE GLOW DISCHARGE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: molecules; line: identification; molecular data; techniques:
spectroscopic
ID SIDE-BAND SPECTROSCOPY; LABORATORY MEASUREMENT; H3O+; H2O+; OH+;
FREQUENCY; ASTRONOMY; SPECTRUM; SOFIA
AB Terahertz absorption spectroscopy was employed to detect the ground-state inversion transitions of the hydronium ion (H3O+). The highly excited ions were created with an extended negative glow discharge through a gas mixture of 1 mtorr of H2O, 2 mtorr of H-2, and 12 mtorr of Ar, which allowed observation of transitions with J and K up to 12. In total, 47 transitions were measured in the 0.9-2.0 THz region and 22 of these were observed for the first time. The experimental uncertainties range from 100 to 300 kHz, which are much better than the range 0.3-1.2 MHz reported in previous work. Differences of up to 25.6 MHz were found between the observed positions and the catalog values that have been used for Herschel data analysis of observations of Sagittarius B2(N), NGC 4418, and Arp 220. The new and improved measurements were fit to experimental accuracies with an updated Hamiltonian, and better H3O+ predictions are reported to support the proper analysis of astronomical observations by high-resolution spectroscopy telescopes, such as Herschel, SOFIA, and ALMA.
C1 [Yu, Shanshan; Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yu, SS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM shanshan.yu@jpl.nasa.gov
RI Yu, Shanshan/D-8733-2016
FU National Science Foundation Graduate Research Fellowship Program [DGE
1144083]; NASA Nancy Grace Roman Fellowship
FX This material is based upon work supported by the National Science
Foundation Graduate Research Fellowship Program under grant No. DGE
1144083. The data presented here were obtained as part of HST Observing
program 12034. K. F. acknowledges support through a NASA Nancy Grace
Roman Fellowship during this work.
NR 21
TC 2
Z9 2
U1 2
U2 10
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 MAY 10
PY 2014
VL 786
IS 2
AR 133
DI 10.1088/0004-637X/786/2/133
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH1MI
UT WOS:000335884500056
ER
PT J
AU Strekalov, DV
Kowligy, AS
Huang, YP
Kumar, P
AF Strekalov, Dmitry V.
Kowligy, Abijith S.
Huang, Yu-Ping
Kumar, Prem
TI Optical sum-frequency generation in a whispering-gallery-mode resonator
SO NEW JOURNAL OF PHYSICS
LA English
DT Article
DE nonlinear optics; sum-frequency generation; whispering-gallery-mode
resonators
ID UP-CONVERSION; MICROCAVITIES
AB We demonstrate sum-frequency generation between a telecom wavelength and the Rb D2 line, achieved through natural phase matching in a nonlinear whispering gallery mode resonator. Due to the strong optical field confinement and ultra high Q of the cavity, the process saturates already at sub-mW pump peak power, at least two orders of magnitude lower than in existing waveguide-based devices. The experimental data are in agreement with the nonlinear dynamics and phase matching theory based on spherical geometry. Our experimental and theoretical results point toward a new platform for manipulating the color and quantum states of light waves for applications such as atomic memory based quantum networking and logic operations with optical signals.
C1 [Strekalov, Dmitry V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kowligy, Abijith S.; Huang, Yu-Ping; Kumar, Prem] Northwestern Univ, Dept EECS, Ctr Photon Commun & Comp, Evanston, IL 60208 USA.
RP Strekalov, DV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM dmitry.v.strekalov@jpl.nasa.gov
RI Kumar, Prem/B-6691-2009
FU DARPA Zeno-based Opto-Electronics program [W31P4Q-09-1-0014]; National
Aeronautics and Space Administration
FX This work was supported by the DARPA Zeno-based Opto-Electronics program
(grant no. W31P4Q-09-1-0014). It was partly carried out at the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with the National Aeronautics and Space Administration. We
thank J U Furst and T Beckmann for useful discussions.
NR 31
TC 13
Z9 13
U1 1
U2 16
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1367-2630
J9 NEW J PHYS
JI New J. Phys.
PD MAY 9
PY 2014
VL 16
AR 053025
DI 10.1088/1367-2630/16/5/053025
PG 15
WC Physics, Multidisciplinary
SC Physics
GA AL0VB
UT WOS:000338843900005
ER
PT J
AU Wiersema, K
Covino, S
Toma, K
van der Horst, AJ
Varela, K
Min, M
Greiner, J
Starling, RLC
Tanvir, NR
Wijers, RAMJ
Campana, S
Curran, PA
Fan, Y
Fynbo, JPU
Gorosabel, J
Gomboc, A
Gotz, D
Hjorth, J
Jin, ZP
Kobayashi, S
Kouveliotou, C
Mundell, C
O'Brien, PT
Pian, E
Rowlinson, A
Russell, DM
Salvaterra, R
Alighieri, SD
Tagliaferri, G
Vergani, SD
Elliott, J
Farina, C
Hartoog, OE
Karjalainen, R
Klose, S
Knust, F
Levan, AJ
Schady, P
Sudilovsky, V
Willingale, R
AF Wiersema, K.
Covino, S.
Toma, K.
van der Horst, A. J.
Varela, K.
Min, M.
Greiner, J.
Starling, R. L. C.
Tanvir, N. R.
Wijers, R. A. M. J.
Campana, S.
Curran, P. A.
Fan, Y.
Fynbo, J. P. U.
Gorosabel, J.
Gomboc, A.
Goetz, D.
Hjorth, J.
Jin, Z. P.
Kobayashi, S.
Kouveliotou, C.
Mundell, C.
O'Brien, P. T.
Pian, E.
Rowlinson, A.
Russell, D. M.
Salvaterra, R.
Alighieri, S. di Serego
Tagliaferri, G.
Vergani, S. D.
Elliott, J.
Farina, C.
Hartoog, O. E.
Karjalainen, R.
Klose, S.
Knust, F.
Levan, A. J.
Schady, P.
Sudilovsky, V.
Willingale, R.
TI Circular polarization in the optical afterglow of GRB 121024A
SO NATURE
LA English
DT Article
ID GAMMA-RAY BURSTS; RELATIVISTIC COLLISIONLESS SHOCKS; MAGNETIC-FIELD
STRUCTURE; LINEAR-POLARIZATION; LIGHT CURVES; EMISSION; POLARIMETRY;
DUST; JETS; EXTINCTION
AB Gamma-ray bursts (GRBs) are most probably powered by collimated relativistic outflows (jets) from accreting black holes at cosmological distances. Bright afterglows are produced when the outflow collides with the ambient medium. Afterglow polarization directly probes the magnetic properties of the jet when measured minutes after the burst, and it probes the geometric properties of the jet and the ambient medium when measured hours to days after the burst(1-5). High values of optical polarization detected minutes after the burst of GRB 120308A indicate the presence of large-scale ordered magnetic fields originating from the central engine(5) (the power source of the GRB). Theoretical models predict low degrees of linear polarization and no circular polarization at late times(6-8), when the energy in the original ejecta is quickly transferred to the ambient medium and propagates farther into the medium as a blast wave. Here we report the detection of circularly polarized light in the afterglow of GRB 121024A, measured 0.15 days after the burst. We show that the circular polarization is intrinsic to the afterglow and unlikely to be produced by dust scattering or plasma propagation effects. A possible explanation is to invoke anisotropic (rather than the commonly assumed isotropic) electron pitch-angle distributions, and we suggest that new models are required to produce the complex microphysics of realistic shocks in relativistic jets(9-11).
C1 [Wiersema, K.; Starling, R. L. C.; Tanvir, N. R.; O'Brien, P. T.; Willingale, R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Covino, S.; Campana, S.; Tagliaferri, G.; Vergani, S. D.] INAF Brera Astron Observ, I-23807 Merate, LC, Italy.
[Toma, K.] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Toma, K.] Tohoku Univ, Astron Inst, Sendai, Miyagi 9808578, Japan.
[Toma, K.] Tohoku Univ, Frontier Res Inst Interdisciplinary Sci, Sendai, Miyagi 9808578, Japan.
[van der Horst, A. J.; Min, M.; Wijers, R. A. M. J.; Rowlinson, A.; Hartoog, O. E.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 SJ Amsterdam, Netherlands.
[Varela, K.; Greiner, J.; Elliott, J.; Knust, F.; Schady, P.; Sudilovsky, V.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Curran, P. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Fan, Y.; Jin, Z. P.] Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, Nanjing 210008, Peoples R China.
[Fynbo, J. P. U.; Hjorth, J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Gorosabel, J.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Gorosabel, J.] Univ Pais Vasco UPV EHU, ETS Ingn, Dept Fis Aplicada, Unidad Asociada Grp Ciencia Planetarias UPV EHU I, E-48013 Bilbao, Spain.
[Gorosabel, J.] Basque Fdn Sci, Ikerbasque, E-48008 Bilbao, Spain.
[Gomboc, A.] Univ Ljubljana, Fac Math & Phys, Ljubljana 1000, Slovenia.
[Goetz, D.] Univ Paris Diderot, CNRS, DSM, AIM UMR CEA 7158,Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Kobayashi, S.; Mundell, C.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, ZP12, Huntsville, AL 35812 USA.
[Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy.
[Pian, E.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Russell, D. M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain.
[Russell, D. M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Russell, D. M.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates.
[Salvaterra, R.] INAF IASF Milano, I-20133 Milan, Italy.
[Alighieri, S. di Serego] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Farina, C.; Karjalainen, R.] Isaac Newton Grp Telescopes, E-38700 Santa Cruz De La Palma, Canary Islands, Spain.
[Klose, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
RP Wiersema, K (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
EM kw113@le.ac.uk
RI Curran, Peter/B-5293-2013; Hjorth, Jens/M-5787-2014;
OI Tagliaferri, Gianpiero/0000-0003-0121-0723; Curran,
Peter/0000-0003-3003-4626; Hjorth, Jens/0000-0002-4571-2306; Salvaterra,
Ruben/0000-0002-9393-8078; Pian, Elena/0000-0001-8646-4858; Russell,
David/0000-0002-3500-631X; Campana, Sergio/0000-0001-6278-1576; Wijers,
Ralph/0000-0002-3101-1808; di Serego Alighieri,
Sperello/0000-0001-8769-2692; Covino, Stefano/0000-0001-9078-5507
FU STFC; JSPS [231446]; European Research Council [247295]; Royal Society
Fellowship; 973 Programme of China [2013CB837000]; Marie Curie Intra
European Fellowship within the 7th European Community [IEF 274805];
Australian Research Council [DP120102393]; UK Space Agency
FX This work is based on observations made with ESO telescopes at the
Paranal Observatory under programme 090.D-0789. We thank all ING staff
for their support of ACAM ToO observations. K. W. thanks J. Hinton for
discussions. K. W. was supported by STFC. K. T. was supported by a JSPS
Research Fellowship for Young Scientists no. 231446. A.J.v.d.H.,
R.A.M.J.W. and A. R. were supported by the European Research Council via
Advanced Investigator grant no. 247295. R. L. C. S. was supported by a
Royal Society Fellowship. Y.F. was supported by the 973 Programme of
China, under grant 2013CB837000. D. M. R. was supported by a Marie Curie
Intra European Fellowship within the 7th European Community Framework
Programme under contract no. IEF 274805. This work was supported by the
Australian Research Council (grant DP120102393). The William Herschel
telescope and its override programme are operated on the island of La
Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de
los Muchachos of the Instituto de Astrofisica de Canarias. This work
made use of data supplied by the UK Swift Science Data Centre at the
University of Leicester, funded by the UK Space Agency.
NR 45
TC 18
Z9 18
U1 0
U2 24
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD MAY 8
PY 2014
VL 509
IS 7499
BP 201
EP +
DI 10.1038/nature13237
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AG5JC
UT WOS:000335454300033
PM 24776800
ER
PT J
AU Ward, RL
Fleddermann, R
Francis, S
Mow-Lowry, C
Wuchenich, D
Elliot, M
Gilles, F
Herding, M
Nicklaus, K
Brown, J
Burke, J
Dligatch, S
Farrant, D
Green, K
Seckold, J
Blundell, M
Brister, R
Smith, C
Danzmann, K
Heinzel, G
Schutze, D
Sheard, BS
Klipstein, W
McClelland, DE
Shaddock, DA
AF Ward, R. L.
Fleddermann, R.
Francis, S.
Mow-Lowry, C.
Wuchenich, D.
Elliot, M.
Gilles, F.
Herding, M.
Nicklaus, K.
Brown, J.
Burke, J.
Dligatch, S.
Farrant, D.
Green, K.
Seckold, J.
Blundell, M.
Brister, R.
Smith, C.
Danzmann, K.
Heinzel, G.
Schuetze, D.
Sheard, B. S.
Klipstein, W.
McClelland, D. E.
Shaddock, D. A.
TI The design and construction of a prototype lateral-transfer
retro-reflector for inter-satellite laser ranging
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
DE satellite interferometry; gravity measurement; precision optics;
satellite optics
AB The Gravity Recovery and Climate Experiment (GRACE) mission, launched in 2002, is nearing an end, and a continuation mission (GRACE Follow-on) is on a fast-tracked development. GRACE Follow-on will include a laser ranging interferometer technology demonstrator, which will perform the first laser interferometric ranging measurement between separate spacecraft. This necessitates the development of lightweight precision optics that can operate in this demanding environment. In particular, this beam routing system, called the triple mirror assembly, for the GRACE Follow-on mission presents a significant manufacturing challenge. Here we report on the design and construction of a prototype triple mirror assembly for the GRACE Follow-on mission. Our constructed prototype has a co-alignment error between the incoming and outgoing beams of 9 mu rad, which meets the requirement that this error must be less than 10 mu rad.
C1 [Ward, R. L.; Fleddermann, R.; Francis, S.; Mow-Lowry, C.; Wuchenich, D.; Elliot, M.; McClelland, D. E.; Shaddock, D. A.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Mow-Lowry, C.; Danzmann, K.; Heinzel, G.; Schuetze, D.; Sheard, B. S.] Leibniz Univ Hannover, Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-30167 Hannover, Germany.
[Mow-Lowry, C.; Heinzel, G.; Schuetze, D.; Sheard, B. S.] Leibniz Univ Hannover, Inst Gravitat Phys, D-30167 Hannover, Germany.
[Gilles, F.; Herding, M.; Nicklaus, K.] SpaceTech GmbH, D-88090 Immenstaad, Germany.
[Brown, J.; Dligatch, S.; Farrant, D.; Green, K.; Seckold, J.] CSIRO, Mat Sci & Engn, Lindfield, NSW 2070, Australia.
[Burke, J.] BIAS, Opt Metrol & Optoelect Syst, D-28359 Bremen, Germany.
[Blundell, M.; Brister, R.; Smith, C.] Mt Stromlo & Siding Spring Observ, EOS Space Syst, Weston, ACT 2611, Australia.
[Klipstein, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ward, RL (reprint author), Australian Natl Univ, GPO Box 4, Canberra, ACT 0200, Australia.
EM robert.ward@anu.edu.au
RI McClelland, David/E-6765-2010; Mow-Lowry, Conor/F-8843-2015; Farrant,
David/A-4028-2008; Shaddock, Daniel/A-7534-2011; Ward,
Robert/I-8032-2014
OI McClelland, David/0000-0001-6210-5842; Shaddock,
Daniel/0000-0002-6885-3494; Ward, Robert/0000-0001-5503-5241
FU German Federal Ministry of Education and Research; Deutsche
Forschungsgemeinschaft (DFG) Cluster of Excellence QUEST (Centre for
Quantum Engineering and Space-Time Research
FX The TMA development was funded by the Australian Space Research Program,
an initiative of the Australian Government, with contributions from the
German Federal Ministry of Education and Research, the German Aerospace
Centre, Australia's Commonwealth Scientific and Industrial Research
Organisation, and the Deutsche Forschungsgemeinschaft (DFG) within the
Cluster of Excellence QUEST (Centre for Quantum Engineering and Space-
Time Research). The authors thank Bill Folkner for invaluable help in
the early stages of the TMA design.
NR 19
TC 7
Z9 8
U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
EI 1361-6382
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD MAY 7
PY 2014
VL 31
IS 9
AR 095015
DI 10.1088/0264-9381/31/9/095015
PG 11
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA AF4HF
UT WOS:000334671900016
ER
PT J
AU Frankenberg, C
O'Dell, C
Berry, J
Guanter, L
Joiner, J
Kohler, P
Pollock, R
Taylor, TE
AF Frankenberg, Christian
O'Dell, Chris
Berry, Joseph
Guanter, Luis
Joiner, Joanna
Koehler, Philipp
Pollock, Randy
Taylor, Thomas E.
TI Prospects for chlorophyll fluorescence remote sensing from the Orbiting
Carbon Observatory-2
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Chlorophyll fluorescence; GPP; OCO; OCO-2; Atmospheric carbon
ID FOURIER-TRANSFORM SPECTROMETER; GASES OBSERVING SATELLITE;
RADIATIVE-TRANSFER MODEL; CO2 RETRIEVAL; SPACE; PHOTOSYNTHESIS; GOSAT;
WATER; PHYTOPLANKTON; SCIAMACHY
AB The Orbiting Carbon Observatory-2 (OCO-2), scheduled to launch in July 2014, is a NASA mission designed to measure atmospheric CO2. Its main purpose is to allow inversions of net flux estimates of CO2 on regional to continental scales using the total column CO2 retrieved using high-resolution spectra in the 0.76, 1.6, and 2.0 mu m ranges. Recently, it was shown that solar-induced chlorophyll fluorescence (SIP), a proxy for gross primary production (GPP, carbon uptake through photosynthesis), can be accurately retrieved from space using high spectral resolution radiances in the 750 nm range from the Japanese GOSAT and European GOME-2 instruments. Here, we use real OCO-2 thermal vacuum test data as well as a full repeat cycle (16 days) of simulated OCO-2 spectra under realistic conditions to evaluate the potential of OCO-2 for retrievals of chlorophyll fluorescence and also its dependence on clouds and aerosols. We find that the single-measurement precision is 03-0.5 Wm(-2)sr(-1) mu m(-1) (15-25% of typical peak values), better than current measurements from space but still difficult to interpret on a single-sounding basis. The most significant advancement will come from smaller ground-pixel sizes and increased measurement frequency, with a 100-fold increase compared to GOSAT (and about 8 times higher than GOME-2). This will largely decrease the need for coarse spatial and temporal averaging in data analysis and pave the way to accurate local studies. We also find that the lack of full global mapping from the OCO-2 only incurs small representativeness errors on regional averages. Eventually, the combination of net ecosystem exchange (NEE) derived from CO2 source/sink inversions and SIF as proxy for GPP from the same satellite will provide a more process-based understanding of the global carbon cycle. (C) 2014 Elsevier Inc. All rights reseved.
C1 [Frankenberg, Christian; Pollock, Randy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[O'Dell, Chris; Taylor, Thomas E.] Colorado State Univ, Ft Collins, CO 80523 USA.
[Berry, Joseph] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA.
[Guanter, Luis; Koehler, Philipp] Free Univ Berlin, Berlin, Germany.
[Joiner, Joanna] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Frankenberg, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Christian.Frankenberg@jpl.nasa.gov
RI Joiner, Joanna/D-6264-2012; Guanter, Luis/I-1588-2015; Frankenberg,
Christian/A-2944-2013
OI Guanter, Luis/0000-0002-8389-5764; Frankenberg,
Christian/0000-0002-0546-5857
FU NASA [1439002]
FX Part of the research 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. (c)
2013. All rights reserved. The Colorado State University contributions
to the ACOS task were supported by NASA contract 1439002. We thank 4
anonymous reviewers for thorough and constructive reviews that
strengthened the manuscript substantially.
NR 43
TC 46
Z9 46
U1 17
U2 133
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAY 5
PY 2014
VL 147
BP 1
EP 12
DI 10.1016/j.rse.2014.02.007
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AH5QR
UT WOS:000336186400001
ER
PT J
AU Mattar, C
Franch, B
Sobrino, JA
Corbari, C
Jimenez-Munoz, JC
Olivera-Guerra, L
Skokovic, D
Soria, G
Oltra-Carrio, R
Julien, Y
Mancini, M
AF Mattar, C.
Franch, B.
Sobrino, J. A.
Corbari, C.
Jimenez-Munoz, J. C.
Olivera-Guerra, L.
Skokovic, D.
Soria, G.
Oltra-Carrio, R.
Julien, Y.
Mancini, M.
TI Impacts of the broadband albedo on actual evapotranspiration estimated
by S-SEBI model over an agricultural area
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Surface broadband albedo; BRDF; AHS; Angular variation; Heat fluxes;
Evapotranspiration; S-SEBI
ID SURFACE-ENERGY BALANCE; EMISSIVITY SEPARATION ALGORITHM; BIDIRECTIONAL
REFLECTANCE MODEL; SPACEBORNE THERMAL EMISSION; LAND-SURFACE; HEAT-FLUX;
HOT-SPOT; DIRECTIONAL SIGNATURES; VEGETATION CANOPY; RADIOMETER ASTER
AB Surface albedo and emissivity are essential variables in surface energy balance. In recent decades, several land surface energy models have used both surface broadband albedo and emissivity in order to achieve reliable evapotranspiration retrievals on a daily basis. Despite these improvements in surface energy models, we noticed an assumption that most studies make when using this framework. It assumes that the surface broadband albedo and emissivity can be estimated directly as a weighted average of spectral surface bi-directional reflectances, and as a weighted average of spectral surface emissivities retrieved at a given view angle, respectively. However, this approach does not take into account surface anisotropy, which is described by the Bi-directional Reflectance Distribution Function (BRDF) in the case of the surface albedo. In this paper, we analyze the influence that estimating land surface albedo directly from the surface reflectance (alpha(REF)) or through the BRDF integration (alpha(BRDF)) has on the estimation of energy balance components (net radiation, latent and sensible heat fluxes and evapotranspiration) by using the Simplified Surface Energy Balance Index (S-SEBI). To this end, in-situ data and remote sensing images acquisitioned at different view zenith angles (VZA) such as 0 degrees, +/- 40 degrees and +/- 57 degrees by the Airborne Hyperspectral Scanner (AHS) over an agricultural area were used. Results show high variation in alpha(REF) depending on the VZA when compared to alpha(BRDF), with the highest difference observed in the backward scattering direction along the hot spot region (RMSE of 0.11 and relative error of 65%). Net radiation gives relative errors from 6 to 17%, with the maximum error obtained in the images that include the hot spot effect, whereas significant changes are not observed in case of the ground heat flux and the evaporative fraction. However, sensible heat flux, latent heat flux and daily evapotranspiration show relative errors ranging between 23-39%, 6-18% and 5-15% respectively. In a future study, the influence of estimating surface emissivity directly from the average of spectral emissivities under a given view angle or using a hemispherical value will be analyzed. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Mattar, C.; Sobrino, J. A.; Jimenez-Munoz, J. C.; Skokovic, D.; Soria, G.; Oltra-Carrio, R.; Julien, Y.] Univ Valencia, Image Proc Lab, Global Change Unit, Valencia 46980, Spain.
[Mattar, C.; Olivera-Guerra, L.] Univ Chile, LAB, Santiago, Chile.
[Franch, B.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Franch, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Corbari, C.; Mancini, M.] Politecn Milan, Dept Civil & Environm Engn, I-20133 Milan, Italy.
RP Mattar, C (reprint author), Univ Valencia, Image Proc Lab, Global Change Unit, Sci Pk,C Catedrtitico Jose Beltran 2, Valencia 46980, Spain.
EM cristian.mattar@uv.es
RI Soria Barres, Guillem/L-9462-2014; Sobrino, Jose/M-1585-2014; Julien,
Yves/M-5224-2014; Mattar, Cristian/P-6711-2014; Jimenez-Munoz, Juan
Carlos/K-2903-2015
OI Soria Barres, Guillem/0000-0002-3148-9238; Sobrino,
Jose/0000-0003-3787-9373; Julien, Yves/0000-0001-5334-7137;
Jimenez-Munoz, Juan Carlos/0000-0001-7562-4895
FU European Union (CEOP-AEGIS) [212921]; Ministerio de Economia y
Competitividad (EODIX) [AYA2008-0595-C04-01]; CEOS-Spain
[AYA2011-29334-C02-01]; Program U-INICIA VID [U-INICIA 4/0612];
Santander Fellowship-University of Chile for young scientist;
Fondecyt-Initial [CONICYT/ref-11130359]
FX We acknowledge funding from the European Union (CEOP-AEGIS, project
FP7-ENV-2007-1 Proposal No. 212921) and the Ministerio de Economia y
Competitividad (EODIX, project AYA2008-0595-C04-01; CEOS-Spain, project
AYA2011-29334-C02-01. This work was also partially funded by Program
U-INICIA VID 2012, grant U-INICIA 4/0612; Santander
Fellowship-University of Chile for young scientist and Fondecyt-Initial
(CONICYT/ref-11130359).
NR 93
TC 12
Z9 12
U1 4
U2 49
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAY 5
PY 2014
VL 147
BP 23
EP 42
DI 10.1016/j.rse.2014.02.011
PG 20
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AH5QR
UT WOS:000336186400003
ER
PT J
AU Gitelson, AA
Peng, Y
Huemmrich, KF
AF Gitelson, Anatoly A.
Peng, Yi
Huemmrich, Karl F.
TI Relationship between fraction of radiation absorbed by photosynthesizing
maize and soybean canopies and NDVI from remotely sensed data taken at
close range and from MODIS 250 m resolution data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Absorbed photosynthetically active radiation; NDVI; Reflectance
ID LEAF-AREA INDEX; PHOTOSYNTHETICALLY ACTIVE RADIATION; GROSS PRIMARY
PRODUCTION; HIGHER-PLANT LEAVES; SPECTRAL REFLECTANCE; CHLOROPHYLL
CONTENT; VEGETATION INDEXES; SOLAR-RADIATION; TRANSFER MODELS; CORN
CANOPIES
AB The fraction of incident photosynthetically active radiation absorbed by the photosynthesizing tissue in a canopy (fAPAR) is a key variable in the assessment of vegetation productivity. It also plays tremendous role in accurate retrieval of light use efficiency, which is essential for assessing vegetation health status. The main goal of this work was to study in detail relationships of fAPAR absorbed by photosynthetically active vegetation (fAPAR(green)) and Normalized Difference Vegetation Index (NDVI) for two crops with contrasting leaf structures (C3 vs. C4) and canopy architectures, using close range (6 m above the canopy) radiometric data and daily MODIS data taken during eight growing seasons over three irrigated and rainfed maize and soybean sites. Our specific goal was to understand differences in fAPAR(green)/NDVI relationship when crop canopy was almost vertically homogeneous (with respect to leaf area and leaf chlorophyll content), as in vegetative stage, and vertically heterogeneous as in reproduction stage. Firstly, we established fAPAR(green)/NDVI relationships for NDVI, taken at close range, and assessed noise equivalent of fAPAR(green) estimation by NDVI, and then we established relationships for NDVI retrieved from daily MODIS 250 m data. Daily MODIS data illuminated fine details of this relationship and detected effects of canopy heterogeneity on fAPAR(green)/NDVI relationship. In vegetative stage, the fAPAR/NDVI relationships for contrasting in leaf structures and canopy architectures crops were almost linear allowing accurate estimation of fAPAR(green) as it is below 0.7. However, very different fAPAR(green)/NDVI relationships in reproductive stages for both crops were observed, showing that canopy architecture and leaf structure greatly affect the relationship as leaf chlorophyll content changes and vertical distribution of chlorophyll content and green LAI inside the canopy becomes heterogeneous. We have found fine details of the fAPAR(green)/NDVI relationships with two types of hysteresis that prevent the use of a single relationship for fAPAR(green) estimation by NDVI over the whole growing season and suggested mechanisms for each type of hysteresis that should be further studied using radiative transfer models. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Gitelson, Anatoly A.; Peng, Yi] Univ NE Lincoln, CALMIT, Sch Nat Resources, Lincoln, NE 68588 USA.
[Huemmrich, Karl F.] Univ MD Baltimore Cty, NASA, Goddard Space Flight Ctr, Joint Ctr Earth Syst Technol, Greenbelt, MD USA.
RP Peng, Y (reprint author), Univ NE Lincoln, CALMIT, Sch Nat Resources, Lincoln, NE 68588 USA.
EM agitelson2@unl.edu
NR 58
TC 18
Z9 22
U1 3
U2 51
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAY 5
PY 2014
VL 147
BP 108
EP 120
DI 10.1016/j.rse.2014.02.014
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AH5QR
UT WOS:000336186400010
ER
PT J
AU Garcia, RA
Fearns, PRCS
McKinna, LIW
AF Garcia, Rodrigo A.
Fearns, Peter R. C. S.
McKinna, Lachlan I. W.
TI Detecting trend and seasonal changes in bathymetry derived from HICO
imagery: A case study of Shark Bay, Western Australia
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE HICO; Hyperspectral; Bathymetry; Change detection; Time series;
Atmospheric correction; Tide correction; Shallow water inversion model;
Propagating uncertainty; Geolocation accuracy
ID GENERALIZED RATIO ASSUMPTION; SHALLOW-WATER BATHYMETRY; OCEAN COLOR;
SEMIANALYTICAL MODEL; COASTAL ZONE; DEPTH; MISREGISTRATION; REFLECTANCE;
RETRIEVAL; SEAGRASS
AB The Hyperspectral Imager for the Coastal Ocean (HICO) aboard the International Space Station has offered for the first time a dedicated space-borne hyperspectral sensor specifically designed for remote sensing of the coastal environment. However, several processing steps are required to convert calibrated top-of-atmosphere radiances to the desired geophysical parameter(s). These steps add various amounts of uncertainty that can cumulatively render the geophysical parameter imprecise and potentially unusable if the objective is to analyze trends and/or seasonal variability. This research presented here has focused on: (1) atmospheric correction of HICO imagery; (2) retrieval of bathymetry using an improved implementation of a shallow water inversion algorithm; (3) propagation of uncertainty due to environmental noise through the bathymetry retrieval process; (4) issues relating to consistent geo-location of HICO imagery necessary for time series analysis, and; (5) tide height corrections of the retrieved bathymetric dataset The underlying question of whether a temporal change in depth is detectable above uncertainty is also addressed. To this end, nine HICO images spanning November 2011 to August 2012, over the Shark Bay World Heritage Area, Western Australia, were examined. The results presented indicate that precision of the bathymetric retrievals is dependent on the shallow water inversion algorithm used. Within this study, an average of 70% of pixels for the entire HICO-derived bathymetry dataset achieved a relative uncertainty of less than +/- 20%. A per-pixel t-test analysis between derived bathymetry images at successive timestamps revealed observable changes in depth to as low as 0.4 m. However, the present geolocation accuracy of HICO is relatively poor and needs further improvements before extensive time series analysis can be performed. (C) 2014 Elsevier Inc All rights reserved.
C1 [Garcia, Rodrigo A.; Fearns, Peter R. C. S.; McKinna, Lachlan I. W.] Curtin Univ, Dept Imaging & Appl Phys, Remote Sensing & Satellite Res Grp, Perth, WA 6845, Australia.
[McKinna, Lachlan I. W.] NASA, Ocean Ecol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Garcia, RA (reprint author), Curtin Univ, Dept Imaging & Appl Phys, Remote Sensing & Satellite Res Grp, GPO Box U1987, Perth, WA 6845, Australia.
EM rodrigo.garcia@postgrad.curtin.edu.au
NR 65
TC 12
Z9 12
U1 2
U2 30
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAY 5
PY 2014
VL 147
BP 186
EP 205
DI 10.1016/j.rse.2014.03.010
PG 20
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AH5QR
UT WOS:000336186400016
ER
PT J
AU Smith, DD
Chang, H
Myneni, K
Rosenberger, AT
AF Smith, David D.
Chang, H.
Myneni, Krishna
Rosenberger, A. T.
TI Fast-light enhancement of an optical cavity by polarization mode
coupling
SO PHYSICAL REVIEW A
LA English
DT Article
ID INDUCED TRANSPARENCY; RESONATOR; SYSTEM; GYROSCOPES
AB We present an entirely linear all-optical method of cavity scale factor enhancement that relies on mode coupling between the orthogonal polarization modes of a single optical cavity, eliminating the necessity of using an atomic medium to produce the required anomalous dispersion, which decreases the dependence of the scale factor on temperature and increases signal-to-noise ratio by reducing absorption and nonlinear effects. The use of a single cavity results in common mode rejection of the noise and drift that would be present in a system of two coupled cavities. We show that the scale-factor-to-mode-width ratio is increased above unity for this system, and demonstrate tuning of the scale factor by (i) directly varying the polarization mode coupling via rotation of an intracavity half-wave plate, and (ii) coherent control of the cavity reflectance which is achieved simply by varying the incident polarization superposition. These tuning methods allow us to closely approach the critical anomalous dispersion condition and achieve unprecedented enhancements in scale factor and in the scale-factor-to-mode-width ratio. Based on these findings, we propose an adaptation of the traditional optical cavity gyroscope that takes advantage of polarization mode coupling to enhance the gyro scale factor, and demonstrate how the bandwidth of the scale factor enhancement for this gyroscope can be effectively broadened in comparison with fast-light gyroscopes based on atomic media.
C1 [Smith, David D.] NASA, George C Marshall Space Flight Ctr, Space Syst Dept, Huntsville, AL 35812 USA.
[Chang, H.] Ducommun Miltec, Huntsville, AL 35806 USA.
[Myneni, Krishna] US Army AMRDEC, RDMR WDS WO, Redstone Arsenal, AL 35898 USA.
[Rosenberger, A. T.] Oklahoma State Univ, Dept Phys, Stillwater, OK 74078 USA.
RP Smith, DD (reprint author), NASA, George C Marshall Space Flight Ctr, Space Syst Dept, ES31, Huntsville, AL 35812 USA.
FU NASA Office of Chief Technologist Game Changing Development Program; U.
S. Army Aviation and Missile Research Development and Engineering Center
(AMRDEC) Missile ST Program; Summer Research and Travel Program of the
Oklahoma State University College of Arts and Sciences
FX This work was sponsored by the NASA Office of Chief Technologist Game
Changing Development Program and the U. S. Army Aviation and Missile
Research Development and Engineering Center (AMRDEC) Missile S&T
Program. The participation of ATR was sponsored by the Summer Research
and Travel Program of the Oklahoma State University College of Arts and
Sciences.
NR 22
TC 15
Z9 15
U1 1
U2 16
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
EI 1094-1622
J9 PHYS REV A
JI Phys. Rev. A
PD MAY 5
PY 2014
VL 89
IS 5
AR 053804
DI 10.1103/PhysRevA.89.053804
PG 9
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA AH4LY
UT WOS:000336100500008
ER
PT J
AU Wuchenich, DMR
Mahrdt, C
Sheard, BS
Francis, SP
Spero, RE
Miller, J
Mow-Lowry, CM
Ward, RL
Klipstein, WM
Heinzel, G
Danzmann, K
McClelland, DE
Shaddock, DA
AF Wuchenich, Danielle M. R.
Mahrdt, Christoph
Sheard, Benjamin S.
Francis, Samuel P.
Spero, Robert E.
Miller, John
Mow-Lowry, Conor M.
Ward, Robert L.
Klipstein, William M.
Heinzel, Gerhard
Danzmann, Karsten
McClelland, David E.
Shaddock, Daniel A.
TI Laser link acquisition demonstration for the GRACE Follow-On mission
SO OPTICS EXPRESS
LA English
DT Article
ID LTP INTERFEROMETER; COMMUNICATION; PHASEMETER; ALIGNMENT; SYSTEM
AB We experimentally demonstrate an inter-satellite laser link acquisition scheme for GRACE Follow-On. In this strategy, dedicated acquisition sensors are not required-instead we use the photodetectors and signal processing hardware already required for science operation. To establish the laser link, a search over five degrees of freedom must be conducted (+/- 3 mrad in pitch/yaw for each laser beam, and +/- 1 GHz for the frequency difference between the two lasers). This search is combined with a FFT-based peak detection algorithm run on each satellite to find the heterodyne beat note resulting when the two beams are interfered. We experimentally demonstrate the two stages of our acquisition strategy: a +/- 3 mrad commissioning scan and a +/- 300 mu rad reacquisition scan. The commissioning scan enables each beam to be pointed at the other satellite to within 142 mu rad of its best alignment point with a frequency difference between lasers of less than 20 MHz. Scanning over the 4 alignment degrees of freedom in our commissioning scan takes 214 seconds, and when combined with sweeping the laser frequency difference at a rate of 88 kHz/s, the entire commissioning sequence completes within 6.3 hours. The reacquisition sequence takes 7 seconds to complete, and optimizes the alignment between beams to allow a smooth transition to differential wavefront sensing-based auto-alignment. (C) 2014 Optical Society of America
C1 [Wuchenich, Danielle M. R.; Francis, Samuel P.; Miller, John; Mow-Lowry, Conor M.; Ward, Robert L.; McClelland, David E.; Shaddock, Daniel A.] Australian Natl Univ, Dept Quantum Sci, Ctr Gravitat Phys, Canberra, ACT 0200, Australia.
[Mahrdt, Christoph; Sheard, Benjamin S.; Heinzel, Gerhard; Danzmann, Karsten] Leibniz Univ Hannover, Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Mahrdt, Christoph; Sheard, Benjamin S.; Heinzel, Gerhard; Danzmann, Karsten] Leibniz Univ Hannover, Inst Gravitat Phys, D-30167 Hannover, Germany.
[Spero, Robert E.; Klipstein, William M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Wuchenich, DMR (reprint author), Australian Natl Univ, Dept Quantum Sci, Ctr Gravitat Phys, Canberra, ACT 0200, Australia.
EM danielle.wuchenich@anu.edu.au
RI McClelland, David/E-6765-2010; Mow-Lowry, Conor/F-8843-2015; Shaddock,
Daniel/A-7534-2011; Ward, Robert/I-8032-2014
OI McClelland, David/0000-0001-6210-5842; Shaddock,
Daniel/0000-0002-6885-3494; Ward, Robert/0000-0001-5503-5241
FU Australian Government; Australian Research Council; "Deutsche
Forschungsgemeinschaft" (DFG) through the Cluster of Excellence QUEST
(Centre for Quantum Engineering and Space-Time Research); National
Aeronautics and Space Administration
FX The authors gratefully acknowledge discussions and advice from Kirk
McKenzie and Andrew Sutton. This work was supported in part under the
Australian Government's Australian Space Research Programme, grants from
the Australian Research Council, and by the "Deutsche
Forschungsgemeinschaft" (DFG) through the Cluster of Excellence QUEST
(Centre for Quantum Engineering and Space-Time Research). Some of the
work described in this paper was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 35
TC 6
Z9 6
U1 1
U2 22
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD MAY 5
PY 2014
VL 22
IS 9
BP 11351
EP 11366
DI 10.1364/OE.22.011351
PG 16
WC Optics
SC Optics
GA AH1TZ
UT WOS:000335905300160
PM 24921832
ER
PT J
AU Collins, MJ
Kirk, JP
Pettit, J
DeGaetano, AT
McCown, MS
Peterson, TC
Means, TN
Zhang, XB
AF Collins, Mathias J.
Kirk, Johnathan P.
Pettit, Joshua
DeGaetano, Arthur T.
McCown, M. Sam
Peterson, Thomas C.
Means, Tiffany N.
Zhang, Xuebin
TI Annual floods in New England (USA) and Atlantic Canada: synoptic
climatology and generating mechanisms
SO PHYSICAL GEOGRAPHY
LA English
DT Article
DE synoptic climatology; hydroclimatology; trends; floods; flood
seasonality
ID NORTHEASTERN UNITED-STATES; WINTER CLIMATE; TRENDS; PRECIPITATION;
20TH-CENTURY; VARIABILITY; MAGNITUDE; FREQUENCY; COAST; OSCILLATION
AB New England and Atlantic Canada are characterized by mixed flood regimes that reflect different storm types, antecedent land surface conditions, and flood seasonality. Mixed flood regimes are known to complicate flood risk analyses, yet the synoptic climatology and precipitation mechanisms that generate annual floods in this region have not been described in detail. We analyzed a set of long-term annual flood records at climate-sensitive stream gauges across the region and classified the synoptic climatology of each annual flood, quantitatively describing the precipitation mechanisms, and characterize flood seasonality. We find that annual floods here are dominantly generated by Great Lakes-sourced storms and Coastal lows, known locally as 'nor'easters.' Great Lakes storms tend to be associated with lower magnitude annual floods (<75th percentile) and Coastal lows are more clearly associated with higher magnitude events (>75th percentile). Tropical cyclones account for few of all annual floods, including extreme events, despite causing some of the region's largest and most destructive floods. Late winter/early spring is when the greatest number of annual floods occur region wide, and rainfall is the dominant flood-producing mechanism. Rainfall in combination with snowmelt is also important. Both mechanisms are expected to be impacted by projected regional climate change. We find little evidence for associations between flood-producing synoptic storm types or precipitation mechanisms and large-scale atmospheric circulation indices or time periods, despite upward trends in New England annual flood magnitudes. To more completely investigate such associations, partial duration flood series that include more floods than just the largest of each year, and their associated synoptic climatologies and precipitation mechanisms, should be analyzed.
C1 [Collins, Mathias J.] NOAA, Natl Marine Fisheries Serv, Gloucester, MA 01930 USA.
[Kirk, Johnathan P.] Kent State Univ, Dept Geog, Kent, OH 44242 USA.
[Pettit, Joshua] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[DeGaetano, Arthur T.] Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY USA.
[McCown, M. Sam; Peterson, Thomas C.] NOAA, Natl Climat Data Ctr, Asheville, NC USA.
[Means, Tiffany N.] Baldwin Grp Inc, Asheville, NC USA.
[Zhang, Xuebin] Environm Canada, Climate Res Div, Toronto, ON, Canada.
RP Collins, MJ (reprint author), NOAA, Natl Marine Fisheries Serv, 55 Great Republ Dr, Gloucester, MA 01930 USA.
EM mathias.collins@noaa.gov
OI Collins, Mathias/0000-0003-4238-2038
FU Cornell University's Department of Earth and Atmospheric Sciences and
Northeast Regional Climate Center; Environment Canada's Climate Research
Division; NOAA Fisheries Office of Habitat Conservation; NOAA's National
Climatic Data Center
FX We thank Cornell University's Department of Earth and Atmospheric
Sciences and Northeast Regional Climate Center, Environment Canada's
Climate Research Division, NOAA Fisheries Office of Habitat
Conservation, and NOAA's National Climatic Data Center for supporting
this project. Numerous staff at Environment Canada and the United States
Geological Survey were responsive to our data requests. William
Armstrong and Zachary Zambreski provided data analysis support. We thank
Associate Editor Brent Yarnal, Katherine Hirschboeck, and two anonymous
referees for thorough reviews that improved the manuscript.
NR 54
TC 10
Z9 10
U1 4
U2 30
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0272-3646
EI 1930-0557
J9 PHYS GEOGR
JI Phys. Geogr.
PD MAY 4
PY 2014
VL 35
IS 3
BP 195
EP 219
DI 10.1080/02723646.2014.888510
PG 25
WC Environmental Sciences; Geography, Physical; Geosciences,
Multidisciplinary; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Physical Geography; Geology;
Meteorology & Atmospheric Sciences
GA AH1EN
UT WOS:000335862700002
ER
PT J
AU Horta, LG
Reaves, MC
AF Horta, Lucas G.
Reaves, Mercedes C.
TI Evaluation of two crew module boilerplate tests using newly developed
calibration metrics
SO INTERNATIONAL JOURNAL OF CRASHWORTHINESS
LA English
DT Article
DE capsule; test calibration; uncertainty analysis; water impact; model
calibration
ID VALIDATION METRICS
AB The paper discusses an application of multi-dimensional calibration metrics to evaluate pressure data from water drop tests of the Max Launch Abort System crew module boilerplate. Specifically, three metrics are discussed: (1) a metric to assess the probability of enveloping the measured data with the model, (2) a multi-dimensional orthogonality metric to assess model adequacy between test and analysis, and (3) a prediction error metric to conduct sensor placement to minimise pressure prediction errors. Data from similar (nearly repeated) capsule drop tests show significant variability in the measured pressure responses. When compared to expected variability using model predictions, it is demonstrated that the measured variability cannot be explained by the model under the current uncertainty assumptions.
C1 [Horta, Lucas G.; Reaves, Mercedes C.] NASA, Langley Res Ctr, Struct Dynam Branch, Hampton, VA 23665 USA.
RP Horta, LG (reprint author), NASA, Langley Res Ctr, Struct Dynam Branch, Hampton, VA 23665 USA.
EM lucas.g.horta@nasa.gov
NR 23
TC 0
Z9 0
U1 0
U2 2
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 1358-8265
EI 1754-2111
J9 INT J CRASHWORTHINES
JI Int. J. Crashworthiness
PD MAY 4
PY 2014
VL 19
IS 3
BP 264
EP 274
DI 10.1080/13588265.2014.883912
PG 11
WC Engineering, Manufacturing; Engineering, Mechanical
SC Engineering
GA AE3MD
UT WOS:000333879700005
ER
PT J
AU Moore, RH
Ziemba, LD
Dutcher, D
Beyersdorf, AJ
Chan, K
Crumeyrolle, S
Raymond, TM
Thornhill, KL
Winstead, EL
Anderson, BE
AF Moore, Richard H.
Ziemba, Luke D.
Dutcher, Dabrina
Beyersdorf, Andreas J.
Chan, Kevin
Crumeyrolle, Suzanne
Raymond, Timothy M.
Thornhill, Kenneth L.
Winstead, Edward L.
Anderson, Bruce E.
TI Mapping the Operation of the Miniature Combustion Aerosol Standard
(Mini-CAST) Soot Generator
SO AEROSOL SCIENCE AND TECHNOLOGY
LA English
DT Article
ID DIESEL EXHAUST PARTICLES; FISCHER-TROPSCH FUELS; HIGH-RESOLUTION;
ORGANIC-CARBON; BLACK CARBON; PARTICULATE-EMISSIONS; HYGROSCOPIC GROWTH;
CATALYTIC STRIPPER; MASS-SPECTROMETER; ACTIVATION
AB The Jing Ltd. miniature combustion aerosol standard (Mini-CAST) soot generator is a portable, commercially available burner that is widely used for laboratory measurements of soot processes. While many studies have used the Mini-CAST to generate soot with known size, concentration, and organic carbon fraction under a single or few conditions, there has been no systematic study of the burner operation over a wide range of operating conditions. Here, we present a comprehensive characterization of the microphysical, chemical, morphological, and hygroscopic properties of Mini-CAST soot over the full range of oxidation air and mixing N-2 flow rates. Very fuel-rich and fuel-lean flame conditions are found to produce organic-dominated soot with mode diameters of 10-60nm, and the highest particle number concentrations are produced under fuel-rich conditions. The lowest organic fraction and largest diameter soot (70-130nm) occur under slightly fuel-lean conditions. Moving from fuel-rich to fuel-lean conditions also increases the O:C ratio of the soot coatings from similar to 0.05 to similar to 0.25, which causes a small fraction of the particles to act as cloud condensation nuclei near the Kelvin limit (kappa similar to 0-10(-3)). Comparison of these property ranges to those reported in the literature for aircraft and diesel engine soots indicates that the Mini-CAST soot is similar to real-world primary soot particles, which lends itself to a variety of process-based soot studies. The trends in soot properties uncovered here will guide selection of burner operating conditions to achieve optimum soot properties that are most relevant to such studies.
Copyright 2014 American Association for Aerosol Research
C1 [Moore, Richard H.; Crumeyrolle, Suzanne] NASA, Langley Res Ctr, Postdoctoral Program, Hampton, VA 30332 USA.
[Moore, Richard H.; Ziemba, Luke D.; Beyersdorf, Andreas J.; Chan, Kevin; Crumeyrolle, Suzanne; Thornhill, Kenneth L.; Winstead, Edward L.; Anderson, Bruce E.] NASA, Langley Res Ctr, Hampton, VA 30332 USA.
[Dutcher, Dabrina; Raymond, Timothy M.] Bucknell Univ, Dept Chem Engn, Lewisburg, PA 17837 USA.
[Thornhill, Kenneth L.; Winstead, Edward L.] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Moore, RH (reprint author), NASA, Langley Res Ctr, 8 Lindbergh Way, Hampton, VA 30332 USA.
EM richard.h.moore@nasa.gov
FU NASA Fundamental Aeronautics and Fixed Wing Programs
FX The authors thank the NASA Fundamental Aeronautics and Fixed Wing
Programs for funding support. The CFD code was developed by A. Nenes
(http://nenes.eas.gatech.edu/CFD).
NR 55
TC 17
Z9 17
U1 3
U2 36
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0278-6826
EI 1521-7388
J9 AEROSOL SCI TECH
JI Aerosol Sci. Technol.
PD MAY 4
PY 2014
VL 48
IS 5
BP 467
EP 479
DI 10.1080/02786826.2014.890694
PG 13
WC Engineering, Chemical; Engineering, Mechanical; Environmental Sciences;
Meteorology & Atmospheric Sciences
SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric
Sciences
GA AE3MO
UT WOS:000333880800002
ER
PT J
AU Raatikainen, T
Lin, JJ
Cerully, KM
Lathem, TL
Moore, RH
Nenes, A
AF Raatikainen, Tomi
Lin, Jack J.
Cerully, Kate M.
Lathem, Terry L.
Moore, Richard H.
Nenes, Athanasios
TI CCN Data Interpretation Under Dynamic Operation Conditions
SO AEROSOL SCIENCE AND TECHNOLOGY
LA English
DT Article
ID SECONDARY ORGANIC AEROSOL; DROPLET GROWTH-KINETICS; ANALYSIS-A METHOD;
ACTIVATION KINETICS; HYGROSCOPICITY; CHAMBER; SPECTRA; COUNTER
AB We have developed a new numerical model for the non-steady-state operation of the Droplet Measurement Technologies (DMT) Cloud Condensation Nuclei (CCN) counter. The model simulates the Scanning Flow CCN Analysis (SFCA) instrument mode, where a wide supersaturation range is continuously scanned by cycling the flow rate over 20-120s. Model accuracy is verified using a broad set of data which include ammonium sulfate calibration data (under conditions of low CCN concentration) and airborne measurements where either the instrument pressure was not controlled or where exceptionally high CCN loadings were observed. It is shown here for the first time that small pressure and flow fluctuations can have a disproportionately large effect on the instrument supersaturation due to localized compressive/expansive heating and cooling. The model shows that, for fast scan times, these effects can explain the observed shape of the SFCA supersaturation-flow calibration curve and transients in the outlet droplet sizes. The extent of supersaturation depletion from the presence of CCN during SFCA operation is also examined; we found that depletion effects can be neglected below 4000cm(-3) for CCN number.
Copyright 2014 American Association for Aerosol Research
C1 [Raatikainen, Tomi; Lin, Jack J.; Lathem, Terry L.; Nenes, Athanasios] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Raatikainen, Tomi] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Cerully, Kate M.; Moore, Richard H.; Nenes, Athanasios] Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA.
[Moore, Richard H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Nenes, A (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, 311 Ferst Dr, Atlanta, GA 30332 USA.
EM nenes@eas.gatech.edu
RI Raatikainen, Tomi/C-5410-2014
FU Finnish Cultural Foundation; DOE STTS grant; DOE GCEP Graduate Research
Environmental and Global Change Education Fellowships; Electrical Power
Research Institute; NSF-CAREER award; NOAA; NSF; Georgia Tech; NASA
FX The authors are grateful for the funding from Finnish Cultural
Foundation, a DOE STTS grant, DOE GCEP Graduate Research Environmental
and Global Change Education Fellowships, the Electrical Power Research
Institute, a NSF-CAREER award, and NOAA, NSF, Georgia Tech, and NASA
grants is acknowledged.
NR 19
TC 3
Z9 3
U1 1
U2 19
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0278-6826
EI 1521-7388
J9 AEROSOL SCI TECH
JI Aerosol Sci. Technol.
PD MAY 4
PY 2014
VL 48
IS 5
BP 552
EP 561
DI 10.1080/02786826.2014.899429
PG 10
WC Engineering, Chemical; Engineering, Mechanical; Environmental Sciences;
Meteorology & Atmospheric Sciences
SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric
Sciences
GA AE3MO
UT WOS:000333880800010
ER
PT J
AU Russell, C
Ding, J
Nunes, A
Lawless, K
AF Russell, Carolyn
Ding, Jeff
Nunes, Arthur
Lawless, Kirby
TI Welding Technology Takes Flight with NASA
SO WELDING JOURNAL
LA English
DT Editorial Material
C1 [Russell, Carolyn; Lawless, Kirby] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Ding, Jeff] NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Welding & Mfg Team, Huntsville, AL 35812 USA.
[Nunes, Arthur] NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL 35812 USA.
RP Russell, C (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM carolyn.k.russell@nasa.gov; robert.j.ding@nasa.gov;
arthurc.nunes@nasa.gov; kirby.g.lawless@nasa.gov
NR 3
TC 0
Z9 0
U1 0
U2 0
PU AMER WELDING SOC
PI MIAMI
PA 550 N W LEJEUNE RD, MIAMI, FL 33126 USA
SN 0043-2296
J9 WELD J
JI Weld. J.
PD MAY
PY 2014
VL 93
IS 5
BP 38
EP 43
PG 6
WC Metallurgy & Metallurgical Engineering
SC Metallurgy & Metallurgical Engineering
GA AW5QR
UT WOS:000346329700005
ER
PT J
AU Miller, RA
Kuczmarski, MA
AF Miller, Robert A.
Kuczmarski, Maria A.
TI Burner Rig for Small Particle Erosion Testing of Thermal Barrier
Coatings
SO JOURNAL OF TESTING AND EVALUATION
LA English
DT Article
DE thermal barrier coatings; erosion; burner rig; computational fluid
dynamics
ID TEMPERATURE; SIMULATION
AB The development of a high-temperature laboratory test to evaluate the erosion resistance of new turbine-blade thermal barrier coatings (TBC) for aircraft gas turbine engines is described. The focus is on improvements to a previously reported design, specifically: (1) larger duct and nozzle diameters leading to a larger and more uniform wear pattern; (2) incorporation of a new auger-style feeder for precise feeding of fine particles at low flow rates; (3) an aperture after the duct to limit the erosive damage at the edges of button specimens; (4) bag filters for particle feed rate measurements. The results of both extensive computational fluid dynamics (CFD) modeling and experiments concentrating on laboratory specimens fabricated from turbine-blade superalloys were used to demonstrate the validity of the test results to meaningfully evaluate the performance of new coating compositions in representative erosive environments, and to help understand damage mechanisms under such conditions. Two specimen geometries were tested in the improved rig using Mach 0.5 jets: "teardrop" burner bar and button specimens. Both types of specimens had electron beam-physical vapor deposition (EB-PVD) prepared ceramic layers of either ZrO2-Y2O3 (7YSZ) or ZrO2-Y2O3-Gd2O3-Yb2O3 (ZYGdYb) applied over PtAl bond coats using various processing parameters or interface treatments. Specimen temperatures for this study were either 980 degrees C (1800 degrees F) or 1090 degrees C (2000 degrees F).
C1 [Miller, Robert A.; Kuczmarski, Maria A.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Miller, RA (reprint author), NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
FU NASA Fundamental Aeronautics Program, Subsonic Rotary Wing Project
FX This work is sponsored by the NASA Fundamental Aeronautics Program,
Subsonic Rotary Wing Project.
NR 36
TC 0
Z9 0
U1 5
U2 16
PU AMER SOC TESTING MATERIALS
PI W CONSHOHOCKEN
PA 100 BARR HARBOR DR, W CONSHOHOCKEN, PA 19428-2959 USA
SN 0090-3973
EI 1945-7553
J9 J TEST EVAL
JI J. Test. Eval.
PD MAY
PY 2014
VL 42
IS 3
BP 648
EP 658
DI 10.1520/JTE20120303
PG 11
WC Materials Science, Characterization & Testing
SC Materials Science
GA AU5JU
UT WOS:000345643800007
ER
PT J
AU Fish, CS
Swenson, CM
Crowley, G
Barjatya, A
Neilsen, T
Gunther, J
Azeem, I
Pilinski, M
Wilder, R
Allen, D
Anderson, M
Bingham, B
Bradford, K
Burr, S
Burt, R
Byers, B
Cook, J
Davis, K
Frazier, C
Grover, S
Hansen, G
Jensen, S
LeBaron, R
Martineau, J
Miller, J
Nelsen, J
Nelson, W
Patterson, P
Stromberg, E
Tran, J
Wassom, S
Weston, C
Whiteley, M
Young, Q
Petersen, J
Schaire, S
Davis, CR
Bokaie, M
Fullmer, R
Baktur, R
Sojka, J
Cousins, M
AF Fish, C. S.
Swenson, C. M.
Crowley, G.
Barjatya, A.
Neilsen, T.
Gunther, J.
Azeem, I.
Pilinski, M.
Wilder, R.
Allen, D.
Anderson, M.
Bingham, B.
Bradford, K.
Burr, S.
Burt, R.
Byers, B.
Cook, J.
Davis, K.
Frazier, C.
Grover, S.
Hansen, G.
Jensen, S.
LeBaron, R.
Martineau, J.
Miller, J.
Nelsen, J.
Nelson, W.
Patterson, P.
Stromberg, E.
Tran, J.
Wassom, S.
Weston, C.
Whiteley, M.
Young, Q.
Petersen, J.
Schaire, S.
Davis, C. R.
Bokaie, M.
Fullmer, R.
Baktur, R.
Sojka, J.
Cousins, M.
TI Design, Development, Implementation, and On-orbit Performance of the
Dynamic Ionosphere CubeSat Experiment Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE DICE; CubeSats; Ionospheric diagnostics; DC and AC electric fields;
Plasma density; IDA4D; AIME; Constellation; Magnetometer; Langmuir probe
ID TOTAL ELECTRON-CONTENT; LATITUDES
AB Funded by the NSF CubeSat and NASA ELaNa programs, the Dynamic Ionosphere CubeSat Experiment (DICE) mission consists of two 1.5U CubeSats which were launched into an eccentric low Earth orbit on October 28, 2011. Each identical spacecraft carries two Langmuir probes to measure ionospheric in-situ plasma densities, electric field probes to measure in-situ DC and AC electric fields, and a science grade magnetometer to measure in-situ DC and AC magnetic fields. Given the tight integration of these multiple sensors with the CubeSat platforms, each of the DICE spacecraft is effectively a "sensor-sat" capable of comprehensive ionospheric diagnostics. The use of two identical sensor-sats at slightly different orbiting velocities in nearly identical orbits permits the de-convolution of spatial and temporal ambiguities in the observations of the ionosphere from a moving platform. In addition to demonstrating nanosat-based constellation science, the DICE mission is advancing a number of groundbreaking CubeSat technologies including miniaturized mechanisms and high-speed downlink communications.
C1 [Fish, C. S.] Utah State Univ, Res Fdn, Space Dynam Lab, North Logan, UT 84341 USA.
[Fish, C. S.] Utah State Univ, Ctr Space Engn, Logan, UT 84322 USA.
[Fish, C. S.] Virginia Tech, Elect & Comp Engn Dept, Blacksburg, VA USA.
[Swenson, C. M.; Gunther, J.; Fullmer, R.; Baktur, R.; Sojka, J.] Utah State Univ, Logan, UT 84322 USA.
[Crowley, G.; Azeem, I.; Pilinski, M.; Wilder, R.] Atmospher & Space Technol Res Associates LLC, Boulder, CO USA.
[Barjatya, A.] Embry Riddle Aeronaut Univ, Daytona Beach, FL USA.
[Neilsen, T.; Allen, D.; Anderson, M.; Bingham, B.; Bradford, K.; Burr, S.; Burt, R.; Byers, B.; Cook, J.; Davis, K.; Frazier, C.; Grover, S.; Hansen, G.; Jensen, S.; LeBaron, R.; Martineau, J.; Miller, J.; Nelsen, J.; Nelson, W.; Patterson, P.; Stromberg, E.; Tran, J.; Wassom, S.; Weston, C.; Whiteley, M.; Young, Q.] Space Dynam Lab, N Logan, UT USA.
[Petersen, J.] L 3 Commun, Salt Lake City, UT USA.
[Schaire, S.] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
[Davis, C. R.] LJT & Associates, Columbia, MD USA.
[Bokaie, M.] TiNi Aerosp, San Rafael, CA USA.
[Cousins, M.] SRI Int, Menlo Pk, CA 94025 USA.
RP Fish, CS (reprint author), Utah State Univ, Res Fdn, Space Dynam Lab, 1695 North Res Pk Way, North Logan, UT 84341 USA.
EM chad.fish@sdl.usu.edu
FU NSF [ATM-0838059, AGS-1212381, AGS-1255782]
FX The authors gratefully acknowledge funding provided by NSF (grant
numbers# ATM-0838059, AGS-1212381, AGS-1255782) and to the NASA ELaNa
III group for launch services. The team would also like to gratefully
acknowledge the countless hours of dedicated and passionate effort from
the students on the DICE program. They indeed rose to the challenge.
Without their energy and consistency, DICE would not have become a
reality.
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAY
PY 2014
VL 181
IS 1-4
BP 61
EP 120
DI 10.1007/s11214-014-0034-x
PG 60
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH2CT
UT WOS:000335929000002
ER
PT J
AU Domingue, DL
Chapman, CR
Killen, RM
Zurbuchen, TH
Gilbert, JA
Sarantos, M
Benna, M
Slavin, JA
Schriver, D
Travnicek, PM
Orlando, TM
Sprague, AL
Blewett, DT
Gillis-Davis, JJ
Feldman, WC
Lawrence, DJ
Ho, GC
Ebel, DS
Nittler, LR
Vilas, F
Pieters, CM
Solomon, SC
Johnson, CL
Winslow, RM
Helbert, J
Peplowski, PN
Weider, SZ
Mouawad, N
Izenberg, NR
McClintock, WE
AF Domingue, Deborah L.
Chapman, Clark R.
Killen, Rosemary M.
Zurbuchen, Thomas H.
Gilbert, Jason A.
Sarantos, Menelaos
Benna, Mehdi
Slavin, James A.
Schriver, David
Travnicek, Pavel M.
Orlando, Thomas M.
Sprague, Ann L.
Blewett, David T.
Gillis-Davis, Jeffrey J.
Feldman, William C.
Lawrence, David J.
Ho, George C.
Ebel, Denton S.
Nittler, Larry R.
Vilas, Faith
Pieters, Carle M.
Solomon, Sean C.
Johnson, Catherine L.
Winslow, Reka M.
Helbert, Joern
Peplowski, Patrick N.
Weider, Shoshana Z.
Mouawad, Nelly
Izenberg, Noam R.
McClintock, William E.
TI Mercury's Weather-Beaten Surface: Understanding Mercury in the Context
of Lunar and Asteroidal Space Weathering Studies
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Mercury (planet); Space weathering; Surface processes; Exosphere;
Surface composition; Space environment
ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; LATE HEAVY BOMBARDMENT; 1ST
MESSENGER FLYBY; ELECTRON-STIMULATED DESORPTION; IRON-SILICATE
FRACTIONATION; MINERAL ABSORPTION FEATURES; ION IRRADIATION EXPERIMENTS;
GAMMA-RAY SPECTROMETER; SOLAR-WIND BOMBARDMENT; NEAR-EARTH ASTEROIDS
AB Mercury's regolith, derived from the crustal bedrock, has been altered by a set of space weathering processes. Before we can interpret crustal composition, it is necessary to understand the nature of these surface alterations. The processes that space weather the surface are the same as those that form Mercury's exosphere (micrometeoroid flux and solar wind interactions) and are moderated by the local space environment and the presence of a global magnetic field. To comprehend how space weathering acts on Mercury's regolith, an understanding is needed of how contributing processes act as an interactive system. As no direct information (e.g., from returned samples) is available about how the system of space weathering affects Mercury's regolith, we use as a basis for comparison the current understanding of these same processes on lunar and asteroidal regoliths as well as laboratory simulations. These comparisons suggest that Mercury's regolith is overturned more frequently (though the characteristic surface time for a grain is unknown even relative to the lunar case), more than an order of magnitude more melt and vapor per unit time and unit area is produced by impact processes than on the Moon (creating a higher glass content via grain coatings and agglutinates), the degree of surface irradiation is comparable to or greater than that on the Moon, and photon irradiation is up to an order of magnitude greater (creating amorphous grain rims, chemically reducing the upper layers of grains to produce nanometer-scale particles of metallic iron, and depleting surface grains in volatile elements and alkali metals). The processes that chemically reduce the surface and produce nanometer-scale particles on Mercury are suggested to be more effective than similar processes on the Moon. Estimated abundances of nanometer-scale particles can account for Mercury's dark surface relative to that of the Moon without requiring macroscopic grains of opaque minerals. The presence of nanometer-scale particles may also account for Mercury's relatively featureless visible-near-infrared reflectance spectra. Characteristics of material returned from asteroid 25143 Itokawa demonstrate that this nanometer-scale material need not be pure iron, raising the possibility that the nanometer-scale material on Mercury may have a composition different from iron metal [such as (Fe,Mg)S]. The expected depletion of volatiles and particularly alkali metals from solar-wind interaction processes are inconsistent with the detection of sodium, potassium, and sulfur within the regolith. One plausible explanation invokes a larger fine fraction (grain size < 45 mu m) and more radiation-damaged grains than in the lunar surface material to create a regolith that is a more efficient reservoir for these volatiles. By this view the volatile elements detected are present not only within the grain structures, but also as adsorbates within the regolith and deposits on the surfaces of the regolith grains. The comparisons with findings from the Moon and asteroids provide a basis for predicting how compositional modifications induced by space weathering have affected Mercury's surface composition.
C1 [Domingue, Deborah L.; Feldman, William C.; Vilas, Faith; Johnson, Catherine L.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Chapman, Clark R.] Southwest Res Inst, Boulder, CO 80302 USA.
[Killen, Rosemary M.; Benna, Mehdi] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Zurbuchen, Thomas H.; Gilbert, Jason A.; Slavin, James A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Sarantos, Menelaos] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Schriver, David] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Travnicek, Pavel M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 90704 USA.
[Orlando, Thomas M.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA.
[Orlando, Thomas M.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Sprague, Ann L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Blewett, David T.; Lawrence, David J.; Ho, George C.; Peplowski, Patrick N.; Izenberg, Noam R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Gillis-Davis, Jeffrey J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Ebel, Denton S.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, Div Phys Sci, York, NY 10023 USA.
[Nittler, Larry R.; Solomon, Sean C.; Weider, Shoshana Z.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Pieters, Carle M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Johnson, Catherine L.; Winslow, Reka M.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z4, Canada.
[Helbert, Joern] DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[Mouawad, Nelly] Lebanese Amer Univ, Dept Nat Sci, Beirut, Lebanon.
[McClintock, William E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
RP Domingue, DL (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
EM domingue@psi.edu
RI Slavin, James/H-3170-2012; Blewett, David/I-4904-2012; Izenberg,
Noam/F-3952-2015; Travnicek, Pavel/G-8608-2014; Ho, George/G-3650-2015;
Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015; Benna,
Mehdi/F-3489-2012; Gilbert, Jason/I-9020-2012;
OI Slavin, James/0000-0002-9206-724X; Blewett, David/0000-0002-9241-6358;
Izenberg, Noam/0000-0003-1629-6478; Ho, George/0000-0003-1093-2066;
Peplowski, Patrick/0000-0001-7154-8143; Lawrence,
David/0000-0002-7696-6667; Gilbert, Jason/0000-0002-3182-7014; Weider,
Shoshana/0000-0003-1034-909X; Helbert, Jorn/0000-0001-5346-9505
FU NASA [NASW-00002, NAS5-97271]; NASA MESSENGER [NNX08AN29G, NNX07AR62GO,
NNX07AR61G, NNX07AR78G]
FX The authors deeply appreciate the efforts and dedication of the
MESSENGER mission operations, engineering, and instrument teams, without
whom the scientific successes of the MESSENGER mission would not have
been possible. The MESSENGER project is supported by the NASA Discovery
Program under contracts NASW-00002 to the Carnegie Institution of
Washington and NAS5-97271 to The Johns Hopkins University Applied
Physics Laboratory. Contributions by D. T. B., D. S., M. B, and R. K.
are made possible by grants from the NASA MESSENGER Participating
Scientist Program (NNX08AN29G, NNX07AR62GO, NNX07AR61G, and NNX07AR78G,
respectively). The authors also thank T. B. McCord and an anonymous
reviewer for their comments on an earlier version of this manuscript.
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD MAY
PY 2014
VL 181
IS 1-4
BP 121
EP 214
DI 10.1007/s11214-014-0039-5
PG 94
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH2CT
UT WOS:000335929000003
ER
PT J
AU Anderson, GE
Gaensler, BM
Kaplan, DL
Slane, PO
Muno, MP
Posselt, B
Hong, J
Murray, SS
Steeghs, DTH
Brogan, CL
Drake, JJ
Farrell, SA
Benjamin, RA
Chakrabarty, D
Drew, JE
Finley, JP
Grindlay, JE
Lazio, TJW
Lee, JC
Mauerhan, JC
van Kerkwijk, MH
AF Anderson, Gemma E.
Gaensler, B. M.
Kaplan, David L.
Slane, Patrick O.
Muno, Michael P.
Posselt, Bettina
Hong, Jaesub
Murray, Stephen S.
Steeghs, Danny T. H.
Brogan, Crystal L.
Drake, Jeremy J.
Farrell, Sean A.
Benjamin, Robert A.
Chakrabarty, Deepto
Drew, Janet E.
Finley, John P.
Grindlay, Jonathan E.
Lazio, T. Joseph W.
Lee, Julia C.
Mauerhan, Jon C.
van Kerkwijk, Marten H.
TI CHASING THE IDENTIFICATION OF ASCA GALACTIC OBJECTS (ChIcAGO): AN X-RAY
SURVEY OF UNIDENTIFIED SOURCES IN THE GALACTIC PLANE. I. SOURCE SAMPLE
AND INITIAL RESULTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE surveys; X-rays: binaries; X-rays: galaxies; X-rays: general; X-rays:
stars
ID XMM-NEWTON OBSERVATIONS; H-II-REGIONS; PULSAR WIND NEBULA; ALL-SKY
SURVEY; SUPERNOVA REMNANT G349.7+0.2; MASSIVE STAR-FORMATION;
MAIN-SEQUENCE STARS; M IR-EXCESS; SOURCE CATALOG; INFRARED COUNTERPART
AB We present the Chasing the Identification of ASCA Galactic Objects (ChIcAGO) survey, which is designed to identify the unknown X-ray sources discovered during the ASCA Galactic Plane Survey (AGPS). Little is known about most of the AGPS sources, especially those that emit primarily in hard X-rays (2-10 keV) within the F-x similar to 10(-13) to 10(-11) erg cm(-2) s(-1) X-ray flux range. In ChIcAGO, the subarcsecond localization capabilities of Chandra have been combined with a detailed multiwavelength follow-up program, with the ultimate goal of classifying the >100 unidentified sources in the AGPS. Overall to date, 93 unidentified AGPS sources have been observed with Chandra as part of the ChIcAGO survey. A total of 253 X-ray point sources have been detected in these Chandra observations within 3' of the original ASCA positions. We have identified infrared and optical counterparts to the majority of these sources, using both new observations and catalogs from existing Galactic plane surveys. X-ray and infrared population statistics for the X-ray point sources detected in the Chandra observations reveal that the primary populations of Galactic plane X-ray sources that emit in the F-x similar to 10(-13) to 10(-11) erg cm(-2) s(-1) flux range are active stellar coronae, massive stars with strong stellar winds that are possibly in colliding wind binaries, X-ray binaries, and magnetars. There is also another primary population that is still unidentified but, on the basis of its X-ray and infrared properties, likely comprises partly Galactic sources and partly active galactic nuclei.
C1 [Anderson, Gemma E.; Gaensler, B. M.; Farrell, Sean A.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia.
[Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA.
[Slane, Patrick O.; Hong, Jaesub; Drake, Jeremy J.; Grindlay, Jonathan E.; Lee, Julia C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Muno, Michael P.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Posselt, Bettina] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Steeghs, Danny T. H.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Brogan, Crystal L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Benjamin, Robert A.] Univ Wisconsin, Dept Phys, Whitewater, WI 53190 USA.
[Chakrabarty, Deepto] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Chakrabarty, Deepto] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Drew, Janet E.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Finley, John P.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Lazio, T. Joseph W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mauerhan, Jon C.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[van Kerkwijk, Marten H.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Anderson, GE (reprint author), Univ Oxford, Dept Phys, Denys Wilkinson Bldg, Oxford OX1 3RH, England.
EM gemma.anderson@astro.ox.ac.uk
RI Lee, Julia/G-2381-2015;
OI Lee, Julia/0000-0002-7336-3588; Anderson, Gemma/0000-0001-6544-8007;
Posselt, Bettina/0000-0003-2317-9747; Gaensler,
Bryan/0000-0002-3382-9558; Drew, Janet/0000-0003-1192-7082; Kaplan,
David/0000-0001-6295-2881
FU Australian Postgraduate Award; Australian Laureate Fellowship through
ARC [FL100100114]; NASA [NAS8-03060, NAS8-39073, GO90155X]; STFC
Advanced Fellowship; Commonwealth of Australia under the International
Science Linkages program; Commonwealth of Australia; Australian Research
Council; Science Foundation for Physics within the University of Sydney;
NFS
FX G.E.A. acknowledges the support of an Australian Postgraduate Award.
B.M.G. acknowledges the support of an Australian Laureate Fellowship
through ARC grant FL100100114. P.O.S. acknowledges partial support from
NASA contract NAS8-03060. D.T.H.S. acknowledges a STFC Advanced
Fellowship. J.J.D. was supported by NASA contract NAS8-39073 to the
Chandra X-ray Center (CXC). Support for this work was also provided by
NASA through Chandra award number GO90155X issued by the CXC, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of NASA. The access to major research facilities program is supported by
the Commonwealth of Australia under the International Science Linkages
program. This research makes use of data obtained with the Chandra X-ray
Observatory and software provided by the CXC in the application packages
CIAO. The ATCA is part of the Australia Telescope, funded by the
Commonwealth of Australia for operation as a National Facility managed
by CSIRO. The MOST is operated with the support of the Australian
Research Council and the Science Foundation for Physics within the
University of Sydney. Observing time on the 6.5 m Baade Magellan
Telescope, located at Las Campanas Observatory, was allocated through
the Harvard-Smithsonian Center for Astrophysics and the Massachusetts
Institute of Technology. 2MASS is a joint project of the University of
Massachusetts and the IPAC/Caltech, funded by NASA and the NFS. GLIMPSE
survey data are part of the Spitzer Legacy Program. The Spitzer Space
Telescope is operated by JPL/Caltech under a contract with NASA. This
research has made use of NASA's Astrophysics Data System.
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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 MAY
PY 2014
VL 212
IS 1
DI 10.1088/0067-0049/212/1/13
PG 35
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL6HG
UT WOS:000339232600013
ER
PT J
AU Ashby, MLN
Stanford, SA
Brodwin, M
Gonzalez, AH
Martinez-Manso, J
Bartlett, JG
Benson, BA
Bleem, LE
Crawford, TM
Dey, A
Dressler, A
Eisenhardt, PRM
Galametz, A
Jannuzi, BT
Marrone, DP
Mei, S
Muzzin, A
Pacaud, F
Pierre, M
Stern, D
Vieira, JD
AF Ashby, M. L. N.
Stanford, S. A.
Brodwin, M.
Gonzalez, A. H.
Martinez-Manso, J.
Bartlett, J. G.
Benson, B. A.
Bleem, L. E.
Crawford, T. M.
Dey, A.
Dressler, A.
Eisenhardt, P. R. M.
Galametz, A.
Jannuzi, B. T.
Marrone, D. P.
Mei, S.
Muzzin, A.
Pacaud, F.
Pierre, M.
Stern, D.
Vieira, J. D.
TI THE SPITZER SOUTH POLE TELESCOPE DEEP FIELD: SURVEY DESIGN AND INFRARED
ARRAY CAMERA CATALOGS (vol 209, 16, 2013)
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Correction
C1 [Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Gonzalez, A. H.; Martinez-Manso, J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Bartlett, J. G.] Univ Paris Diderot, CEA IRFU, Observ Paris, Sorbonne Paris Cite,CNRS IN2P3, F-75205 Paris 13, France.
[Benson, B. A.; Bleem, L. E.; Crawford, T. M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bleem, L. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Crawford, T. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Dey, A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Dressler, A.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Eisenhardt, P. R. M.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Galametz, A.] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy.
[Jannuzi, B. T.; Marrone, D. P.] Univ Arizona, Dept Astron, Tucson, AZ 85719 USA.
[Jannuzi, B. T.; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA.
[Mei, S.] Observ Paris, GEPI, Sect Meudon, F-92190 Meudon, France.
[Mei, S.] Univ Paris Denis Diderot, F-75205 Paris 13, France.
[Mei, S.] Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Muzzin, A.] Leiden Univ, Leiden Observ, NL-9513 RA Leiden, Netherlands.
[Pacaud, F.] Argelander Inst Astron, D-53121 Bonn, Germany.
[Pierre, M.] AIM IRFU DSM CEA, Serv Astrophys, F-91190 Gif Sur Yvette, France.
[Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
RP Ashby, MLN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mashby@cfa.harvard.edu
NR 1
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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 MAY
PY 2014
VL 212
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AR 16
DI 10.1088/0067-0049/212/1/16
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL6HG
UT WOS:000339232600016
ER
PT J
AU Mandelbaum, R
Rowe, B
Bosch, J
Chang, C
Courbin, F
Gill, M
Jarvis, M
Kannawadi, A
Kacprzak, T
Lackner, C
Leauthaud, A
Miyatake, H
Nakajima, R
Rhodes, J
Simet, M
Zuntz, J
Armstrong, B
Bridle, S
Coupon, J
Dietrich, JP
Gentile, M
Heymans, C
Jurling, AS
Kent, SM
Kirkby, D
Margala, D
Massey, R
Melchior, P
Peterson, J
Roodman, A
Schrabback, T
AF Mandelbaum, Rachel
Rowe, Barnaby
Bosch, James
Chang, Chihway
Courbin, Frederic
Gill, Mandeep
Jarvis, Mike
Kannawadi, Arun
Kacprzak, Tomasz
Lackner, Claire
Leauthaud, Alexie
Miyatake, Hironao
Nakajima, Reiko
Rhodes, Jason
Simet, Melanie
Zuntz, Joe
Armstrong, Bob
Bridle, Sarah
Coupon, Jean
Dietrich, Jorg P.
Gentile, Marc
Heymans, Catherine
Jurling, Alden S.
Kent, Stephen M.
Kirkby, David
Margala, Daniel
Massey, Richard
Melchior, Peter
Peterson, John
Roodman, Aaron
Schrabback, Tim
TI THE THIRD GRAVITATIONAL LENSING ACCURACY TESTING (GREAT3) CHALLENGE
HANDBOOK
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE gravitational lensing: weak; methods: data analysis; methods:
statistical; techniques: image processing
ID HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; IMAGE-ANALYSIS COMPETITION;
COSMIC SHEAR MEASUREMENT; POINT-SPREAD FUNCTION; ATMOSPHERIC-TURBULENCE;
ADVANCED CAMERA; DARK-MATTER; SHAPE MEASUREMENTS; POLAR SHAPELETS
AB The GRavitational lEnsing Accuracy Testing 3 (GREAT3) challenge is the third in a series of image analysis challenges, with a goal of testing and facilitating the development of methods for analyzing astronomical images that will be used to measure weak gravitational lensing. This measurement requires extremely precise estimation of very small galaxy shape distortions, in the presence of far larger intrinsic galaxy shapes and distortions due to the blurring kernel caused by the atmosphere, telescope optics, and instrumental effects. The GREAT3 challenge is posed to the astronomy, machine learning, and statistics communities, and includes tests of three specific effects that are of immediate relevance to upcoming weak lensing surveys, two of which have never been tested in a community challenge before. These effects include many novel aspects including realistically complex galaxy models based on high-resolution imaging from space; a spatially varying, physically motivated blurring kernel; and a combination of multiple different exposures. To facilitate entry by people new to the field, and for use as a diagnostic tool, the simulation software for the challenge is publicly available, though the exact parameters used for the challenge are blinded. Sample scripts to analyze the challenge data using existing methods will also be provided.
C1 [Mandelbaum, Rachel; Kannawadi, Arun; Simet, Melanie] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Rowe, Barnaby; Kacprzak, Tomasz] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Rowe, Barnaby; Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bosch, James; Miyatake, Hironao] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Chang, Chihway; Gill, Mandeep; Roodman, Aaron] Stanford Univ, KIPAC, Stanford, CA 94309 USA.
[Courbin, Frederic; Gentile, Marc] EPFL, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland.
[Jarvis, Mike; Armstrong, Bob] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Lackner, Claire; Leauthaud, Alexie] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba, Japan.
[Nakajima, Reiko; Schrabback, Tim] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA.
[Zuntz, Joe; Bridle, Sarah] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Coupon, Jean] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Dietrich, Jorg P.] Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Dietrich, Jorg P.] Excellence Cluster Universe, D-85748 Munich, Germany.
[Heymans, Catherine] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Jurling, Alden S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jurling, Alden S.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14618 USA.
[Kent, Stephen M.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Kirkby, David; Margala, Daniel] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Massey, Richard] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[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.
[Peterson, John] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
RP Mandelbaum, R (reprint author), Carnegie Mellon Univ, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.
RI Mandelbaum, Rachel/N-8955-2014; Simet, Melanie/A-3415-2016; EPFL,
Physics/O-6514-2016;
OI Mandelbaum, Rachel/0000-0003-2271-1527; Simet,
Melanie/0000-0001-8823-8926; Kirkby, David/0000-0002-8828-5463;
Dietrich, Jorg/0000-0002-8134-9591; Rowe, Barnaby/0000-0002-7042-9174
FU National Science Foundation [PHYS-1066293]; NASA via the Strategic
University Research Partnership (SURP) Program of the Jet Propulsion
Laboratory, California Institute of Technology; IST Programme of the
European Community under the PASCAL2 Network of Excellence
[IST-2007-216886]; NASA through Space Telescope Science Institute; NASA
[NAS5-26555]; European Research Council [240672, 240185]; JSPS
Postdoctoral Fellowships for Research Abroad; Swiss National Science
Foundation (SNSF); LLC [De-AC02-07CH11359]; United States Department of
Energy; [HST-AR-12857.01-A]
FX The authors of this work benefited greatly from discussions with
Christopher Hirata, Gary Bernstein, Lance Miller, and Erin Sheldon; the
WFIRST project office, including David Content; the Euclid Consortium;
and the LSST imSim team, including En-Hsin Peng; and Peter Freeman. We
thank the PASCAL-2 network for its sponsorship of the challenge. This
work was supported in part by the National Science Foundation under
grant No. PHYS-1066293 and the hospitality of the Aspen Center for
Physics.; This project was supported in part by NASA via the Strategic
University Research Partnership (SURP) Program of the Jet Propulsion
Laboratory, California Institute of Technology; and by the IST Programme
of the European Community, under the PASCAL2 Network of Excellence,
IST-2007-216886. This article only reflects the authors' views.; R.M.
was supported in part by program HST-AR-12857.01-A, provided by NASA
through a grant from the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Incorporated, under NASA contract NAS5-26555. B.R. and S.B. acknowledge
support from the European Research Council in the form of a Starting
Grant with number 240672. H.M. acknowledges support from JSPS
Postdoctoral Fellowships for Research Abroad. C.H. acknowledges support
from the European Research Council under the EC FP7 grant number 240185.
F.C. and M.G. are supported by the Swiss National Science Foundation
(SNSF).; Center for Particle Astrophysics, Fermi National Accelerator
Laboratory is operated by Fermi Research Alliance, LLC under contract
No. De-AC02-07CH11359 with the United States Department of Energy.
NR 100
TC 37
Z9 37
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAY
PY 2014
VL 212
IS 1
AR 5
DI 10.1088/0067-0049/212/1/5
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL6HG
UT WOS:000339232600005
ER
PT J
AU Downs, ME
Buxton, R
Moore, A
Ploutz-Snyder, R
Ploutz-Snyder, L
AF Downs, Meghan E.
Buxton, Roxanne
Moore, Alan, Jr.
Ploutz-Snyder, Robert
Ploutz-Snyder, Lori
TI Contributions Of Astronauts Aerobic Exercise Intensity And Time On
Change In Vo(2)Peak During Spaceflight
SO MEDICINE AND SCIENCE IN SPORTS AND EXERCISE
LA English
DT Meeting Abstract
CT 61st Annual Meeting of the American-College-of-Sports-Medicine
CY APR 01-04, 2014
CL Atlanta, GA
SP Amer Coll Sports Med
C1 [Downs, Meghan E.; Buxton, Roxanne; Moore, Alan, Jr.; Ploutz-Snyder, Robert; Ploutz-Snyder, Lori] NASA JSC, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 1
U2 4
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 0195-9131
EI 1530-0315
J9 MED SCI SPORT EXER
JI Med. Sci. Sports Exerc.
PD MAY
PY 2014
VL 46
IS 5
SU 1
MA 1578
BP 429
EP 430
PG 3
WC Sport Sciences
SC Sport Sciences
GA AL4PW
UT WOS:000339115903023
ER
PT J
AU Moore, AD
Downs, ME
Lee, SMC
Feiveson, AH
Knudsen, P
Evetts, SE
Ploutz-Snyder, L
AF Moore, Alan D., Jr.
Downs, Meghan E.
Lee, Stuart M. C.
Feiveson, Alan H.
Knudsen, Poul
Evetts, Simon E.
Ploutz-Snyder, Lori
TI Peak Oxygen Uptake During And After Long-duration Space Flight
SO MEDICINE AND SCIENCE IN SPORTS AND EXERCISE
LA English
DT Meeting Abstract
CT 61st Annual Meeting of the American-College-of-Sports-Medicine
CY APR 01-04, 2014
CL Atlanta, GA
SP Amer Coll Sports Med
C1 [Moore, Alan D., Jr.; Lee, Stuart M. C.] Wyle Sci Technol & Engn, Houston, TX USA.
[Downs, Meghan E.] Univ Houston, Houston, TX USA.
[Feiveson, Alan H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Knudsen, Poul] Danish Aerosp Co, Odense, Denmark.
[Evetts, Simon E.] Wyle GmbH, Cologne, Germany.
[Ploutz-Snyder, Lori] Univ Space Res Assoc, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 0195-9131
EI 1530-0315
J9 MED SCI SPORT EXER
JI Med. Sci. Sports Exerc.
PD MAY
PY 2014
VL 46
IS 5
SU 1
MA 1577
BP 429
EP 429
PG 1
WC Sport Sciences
SC Sport Sciences
GA AL4PW
UT WOS:000339115903022
ER
PT J
AU Hou, AY
Kakar, RK
Neeck, S
Azarbarzin, AA
Kummerow, CD
Kojima, M
Oki, R
Nakamura, K
Iguchi, T
AF Hou, Arthur Y.
Kakar, Ramesh K.
Neeck, Steven
Azarbarzin, Ardeshir A.
Kummerow, Christian D.
Kojima, Masahiro
Oki, Riko
Nakamura, Kenji
Iguchi, Toshio
TI THE GLOBAL PRECIPITATION MEASUREMENT MISSION
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID DATA ASSIMILATION SYSTEM; PASSIVE MICROWAVE OBSERVATIONS; RAIN-PROFILING
ALGORITHM; DUAL-WAVELENGTH RADAR; TROPICAL RAINFALL; RETRIEVAL
ALGORITHM; BAYESIAN-ESTIMATION; TRMM SATELLITE; RADIOMETER; IMPACT
AB Precipitation affects many aspects of our everyday life. It is the primary source of freshwater and has significant socioeconomic impacts resulting from natural hazards such as hurricanes, floods, droughts, and landslides. Fundamentally, precipitation is a critical component of the global water and energy cycle that governs the weather, climate, and ecological systems. Accurate and timely knowledge of when, where, and how much it rains or snows is essential for understanding how the Earth system functions and for improving the prediction of weather, climate, freshwater resources, and natural hazard events.
The Global Precipitation Measurement (GPM) mission is an international satellite mission specifically designed to set a new standard for the measurement of precipitation from space and to provide a new generation of global rainfall and snowfall observations in all parts of the world every 3 h. The National Aeronautics and Space Administration (NASA) and the Japan Aerospace and Exploration Agency (JAXA) successfully launched the Core Observatory satellite on 28 February 2014 carrying advanced radar and radiometer systems to serve as a precipitation physics observatory. This will serve as a transfer standard for improving the accuracy and consistency of precipitation measurements from a constellation of research and operational satellites provided by a consortium of international partners. GPM will provide key measurements for understanding the global water and energy cycle in a changing climate as well as timely information useful for a range of regional and global societal applications such as numerical weather prediction, natural hazard monitoring, freshwater resource management, and crop forecasting.
C1 [Hou, Arthur Y.; Azarbarzin, Ardeshir A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kakar, Ramesh K.; Neeck, Steven] Natl Aeronaut & Space Adm Headquarters, Washington, DC USA.
[Kummerow, Christian D.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Kojima, Masahiro] Japan Aerosp Explorat Agcy, Tsukuba Space Ctr, Tsukuba, Ibaraki 3058505, Japan.
[Oki, Riko] Japan Aerosp Explorat Agcy, Earth Observat Res Ctr, Tsukuba, Ibaraki, Japan.
[Nakamura, Kenji] Dokkyo Univ, Dept Econ Sustainabil, Saitama, Japan.
[Iguchi, Toshio] Natl Inst Informat & Commun Technol, Tokyo, Japan.
RP Kummerow, CD (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
EM kummerow@atmos.colostate.edu
RI Measurement, Global/C-4698-2015; PMM, JAXA/K-8537-2016
FU NASA Earth Science Division Flight Programs
FX The authors thank Christopher Kidd, Eric Wood, and Gail
Skofronick-Jackson for valuable comments on the manuscript. It is also a
pleasure to acknowledge contributions to this article by members of the
NASA PMM Science Team, the JAXA PMM Science Team, the NASA GPM Advisory
Panel on Ground Validation, the GMI Calibration Task Force, the GMI
High-Frequency Channels Advisory Group, the U.S.-Japan CEOS
Precipitation Constellation Study Team, and the GPM Flight Project at
NASA Goddard Space Flight Center in particular, Robert Adler, Emmanouil
Anagnostou, Ana Barros, Peter Bauer, Rafael Bras, Scott Braun, Candace
Carlisle, V. Chandrasekar, John Durning, Ralph Ferraro, Kinji Furukawa,
Efi Foufoula-Georgiou, Ziad Haddad, Steve Horowitz, Robert Houze, David
Hudak, George Huffman, Paul Joe, Linwood Jones, Dalia Kirschbaum, Jarkko
Koskinen, Sergey Krimchansky, William Lau, Dennis Lettenmaier, Vincenzo
Levizzani, Xin Lin, Guosheng Liu, Robert Meneghini, Joe Munchak, William
Olson, Christa Peters-Lidard, Walter Petersen, Fritz Policelli, Didier
Renaut, Remy Roca, Christopher Ruf, Steven Rutledge, Mathew Schwaller,
Marshall Shepherd, James Shiue, Eric Smith, Soroosh Sorooshian, Erich
Stocker, Wei-Kuo Tao, Joe Turk, Fuzhong Weng, Thomas Wilheit, and Edward
Zipser. This work is supported by NASA Earth Science Division Flight
Programs.
NR 89
TC 221
Z9 223
U1 20
U2 111
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 MAY
PY 2014
VL 95
IS 5
BP 701
EP +
DI 10.1175/BAMS-D-13-00164.1
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AL4GS
UT WOS:000339091500008
ER
PT J
AU Ploutz-Snyder, RJ
Fiedler, J
Feiveson, AH
AF Ploutz-Snyder, Robert J.
Fiedler, James
Feiveson, Alan H.
TI Justifying small-n research in scientifically amazing settings:
challenging the notion that only "big-n" studies are worthwhile
SO JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Editorial Material
ID CONFIDENCE-INTERVALS; SAMPLE-SIZE; INFORMATION; DESIGN
C1 [Ploutz-Snyder, Robert J.; Fiedler, James; Feiveson, Alan H.] NASA Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA.
RP Ploutz-Snyder, RJ (reprint author), NASA Johnson Space Ctr, Univ Space Res Assoc, 2101 NASA Pkwy,Mail Code SK3, Houston, TX 77058 USA.
EM Robert.ploutz-snyder-1@nasa.gov
NR 10
TC 5
Z9 6
U1 0
U2 7
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 8750-7587
EI 1522-1601
J9 J APPL PHYSIOL
JI J. Appl. Physiol.
PD MAY
PY 2014
VL 116
IS 9
BP 1251
EP 1252
DI 10.1152/japplphysiol.01335.2013
PG 2
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA AL5IO
UT WOS:000339167300017
PM 24408991
ER
PT J
AU Ploutz-Snyder, RJ
Fiedler, J
Feiveson, AH
AF Ploutz-Snyder, Robert J.
Fiedler, James
Feiveson, Alan H.
TI Last Word on Viewpoint: Justifying small-n research in scientifically
amazing settings: Challenging the notion that only "big-n" studies are
worthwhile
SO JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Letter
C1 [Ploutz-Snyder, Robert J.; Fiedler, James; Feiveson, Alan H.] NASA Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA.
RP Ploutz-Snyder, RJ (reprint author), NASA Johnson Space Ctr, Univ Space Res Assoc, 2101 NASA Pkwy,Mail Code SK3, Houston, TX 77058 USA.
EM Robert.ploutz-snyder-1@nasa.gov
NR 2
TC 0
Z9 0
U1 0
U2 3
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 8750-7587
EI 1522-1601
J9 J APPL PHYSIOL
JI J. Appl. Physiol.
PD MAY
PY 2014
VL 116
IS 9
BP 1254
EP 1254
DI 10.1152/japplphysiol.00214.2014
PG 1
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA AL5IO
UT WOS:000339167300020
PM 24789885
ER
PT J
AU Garrison, JL
Cardellach, E
Gleason, S
Katzberg, S
AF Garrison, James L.
Cardellach, Estel
Gleason, Scott
Katzberg, Steve
TI Foreword to Special Issue on Reflectometry using Global Navigation
Satellite Systems and Other Signals of Opportunity (GNSS+R)
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Editorial Material
ID REFLECTED GPS SIGNALS; OCEAN ALTIMETRY; WIND-SPEED
C1 [Garrison, James L.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
[Cardellach, Estel] Inst Ciencies Espai CSIC IEEC, Barcelona 08193, Spain.
[Gleason, Scott] Southwest Res Inst, Boulder, CO 80302 USA.
[Katzberg, Steve] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Garrison, JL (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
RI Cardellach, Estel/C-9418-2012
OI Cardellach, Estel/0000-0001-8908-0972
NR 40
TC 3
Z9 3
U1 0
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD MAY
PY 2014
VL 7
IS 5
SI SI
BP 1412
EP 1415
DI 10.1109/JSTARS.2014.2325996
PG 4
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA AJ7TQ
UT WOS:000337900700001
ER
PT J
AU Lowe, ST
Meehan, T
Young, L
AF Lowe, Stephen T.
Meehan, Thomas
Young, Larry
TI Direct Signal Enhanced Semicodeless Processing of GNSS Surface-Reflected
Signals
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Altimetry; bistatic radar; global navigation satellite systems (GNSS)
reflectometry; global positioning system (GPS) reflectometry;
scatterometry; semicodeless signal processing
ID SEA-SURFACE; OCEAN; REFLECTOMETRY; ALTIMETRY; PARIS
AB This paper presents an aircraft demonstration of direct-signal enhanced semicodeless processing of global navigation satellite systems (GNSS) signals reflected from the Earth's surface. Comparisons are made between this new method and an interferometric approach to GNSS reflectometry. Results show that this technique produces waveforms with greater signal-to-noise compared with the interferometric approach for all GNSS signals currently in use or planned for the near future. Alternatively, the semicodeless technique can have similar performance with smaller antennas for lower hardware costs. The semicodeless approach also has the advantage that different signals along with their different surface spatial resolutions are processed separately, each signal's coherent integration time can be optimized, and ground/aircraft experiments and tests are free of spurious signals. The signal processing demands of the semicodeless approach are shown to be proportional to the number of signal components processed when integrated with a GNSS precise orbit determination (POD) receiver.
C1 [Lowe, Stephen T.; Meehan, Thomas; Young, Larry] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lowe, ST (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM steve.lowe@jpl.nasa.gov; tomas.meehan@jpl.nasa.gov;
larry.young-@jpl.nasa.gov
FU National Aeronautics and Space Administration; NASA's Physical
Oceanography Program
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, CA, USA, under a contract with the
National Aeronautics and Space Administration. This work was supported
in part by John LaBrecque, Lead, Earth Surface and Interior Focus Area,
NASA's Science Mission Directorate. The Monterey Bay aircraft
experiments were originally funded under NASA's Physical Oceanography
Program. Government sponsorship acknowledged.
NR 15
TC 9
Z9 9
U1 0
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD MAY
PY 2014
VL 7
IS 5
SI SI
BP 1469
EP 1472
DI 10.1109/JSTARS.2014.2313061
PG 4
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA AJ7TQ
UT WOS:000337900700007
ER
PT J
AU Przekop, A
Jegley, DC
AF Przekop, Adam
Jegley, Dawn C.
TI Evaluation of a Metallic Repair on a Rod-Stiffened Composite Panel
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 54th AIAA/ASME/ASCE/AHS/ASC Structures, Structural Dynamics, and
Materials Conference
CY APR 08-11, 2013
CL Boston, MA
SP AIAA, ASME, ASCE, AHS, ASC
AB A design and analysis of a repair concept applicable to a stiffened composite panel based on the pultruded rod stitched efficient unitized structure was recently completed. The damage scenario considered was a midbay-to-midbay saw-cut with a severed stiffener, flange, and skin. Advanced modeling techniques such as mesh-independent definition of compliant fasteners and elastic-plastic material properties for metal parts were used in the finite-element analysis supporting the design effort. A bolted metallic repair was selected so that it could be easily applied in the operational environment. The present work describes results obtained from a tension panel test conducted to validate both the repair concept and finite-element analysis techniques used in the design effort. The test proved that the proposed repair concept is capable of sustaining load levels that are higher than those resulting from the current working stress allowables. This conclusion enables upward revision of the stress allowables that had been kept at an overly conservative level due to concerns associated with repairability of the panels. Correlation of test data with finite-element analysis results is also presented and assessed.
C1 [Przekop, Adam] Analyt Mech Associates Inc, NASA Langley Res Ctr, Hampton, VA 23666 USA.
[Jegley, Dawn C.] NASA Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
RP Przekop, A (reprint author), Analyt Mech Associates Inc, NASA Langley Res Ctr, Mail Stop 190, Hampton, VA 23666 USA.
NR 16
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD MAY-JUN
PY 2014
VL 51
IS 3
BP 792
EP 804
DI 10.2514/1.C032461
PG 13
WC Engineering, Aerospace
SC Engineering
GA AJ8UT
UT WOS:000337984100008
ER
PT J
AU Arntzen, M
Rizzi, SA
Visser, HG
Simon, DG
AF Arntzen, Michael
Rizzi, Stephen A.
Visser, Hendrikus G.
Simon, Dick G.
TI Framework for Simulating Aircraft Flyover Noise Through Nonstandard
Atmospheres
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 18th AIAA/CEAS Aeroacoustics Conference / 33rd AIAA Aeroacoustics
Conference
CY JUN 04-06, 2012
CL Colorado Springs, CO
SP AIAA, CEAS
AB This paper describes a new framework for the synthesis of aircraft flyover noise through a nonstandard atmosphere. Central to the framework is a ray-tracing algorithm that defines multiple curved propagation paths, if the atmosphere allows, between the moving source and listener. Because each path has a different emission angle, synthesis of the sound at the source must be performed independently for each path. The time delay, spreading loss, and absorption (ground and atmosphere) are integrated along each path and applied to each synthesized aircraft noise source to simulate a flyover. A final step assigns each resulting signal to its corresponding receiver angle for the simulation of a flyover in a virtual reality environment. Spectrograms of the results from a straight path and a curved path modeling assumption are shown. When the aircraft is at close range, the straight path results are valid. Differences appear especially when the source is relatively far away at shallow elevation angles. These differences, however, are not significant in common sound metrics. Although the framework used in this work performs off-line processing, it is conducive to real-time implementation.
C1 [Arntzen, Michael] Natl Aerosp Lab, NL-1059 CM Amsterdam, Netherlands.
[Rizzi, Stephen A.] NASA Langley Res Ctr, Struct Acoust Branch, MS 463, Hampton, VA 23681 USA.
[Visser, Hendrikus G.; Simon, Dick G.] Delft Univ Technol, NL-2600 AA Delft, Netherlands.
RP Arntzen, M (reprint author), Natl Aerosp Lab, Anthony Fokkerweg 2, NL-1059 CM Amsterdam, Netherlands.
OI Visser, Hendrikus/0000-0002-5644-0430
NR 30
TC 4
Z9 4
U1 0
U2 0
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 MAY-JUN
PY 2014
VL 51
IS 3
BP 956
EP 966
DI 10.2514/1.C032049
PG 11
WC Engineering, Aerospace
SC Engineering
GA AJ8UT
UT WOS:000337984100024
ER
PT J
AU Park, MA
Aftosmis, MJ
Campbell, RL
Carter, MB
Cliff, SE
Bangert, LS
AF Park, Michael A.
Aftosmis, Michael J.
Campbell, Richard L.
Carter, Melissa B.
Cliff, Susan E.
Bangert, Linda S.
TI Summary of the 2008 NASA Fundamental Aeronautics Program Sonic Boom
Prediction Workshop
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 51st AIAA Aerospace Sciences Meeting and Exhibit Including the New
Horizons Forum and Aerospace Exposition
CY JAN 06-10, 2013
CL Grapevine, TX
SP AIAA
ID COMPUTATIONAL FLUID-DYNAMICS; POSTERIORI ERROR ESTIMATION;
FINITE-ELEMENT METHODS; GRID ADAPTATION; FUNCTIONAL OUTPUTS; MESH
GENERATION; FLOWS
AB The Supersonics Project of the NASA Fundamental Aeronautics Program organized an internal sonic boom workshop to evaluate near-field sonic-boom prediction capability at the Fundamental Aeronautics Annual Meeting in Atlanta, Georgia, on 8 October 2008. Workshop participants computed sonic-boom signatures for three nonlifting bodies and two lifting configurations. Cone cylinder, parabolic, and quartic bodies of revolution comprised the nonlifting cases. The lifting configurations were a simple 69 deg delta-wing body and a complete low-boom transport configuration designed during the High Speed Research Project in the 1990s with wing, body, tail, nacelle, and boundary-layer diverter components. The AIRPLANE, Cart3D, FUN3D, and USM3D flow solvers were employed with the ANET signature propagation tool, output-based adaptation, and a priori adaptation based on freestream Mach number and angle of attack. Results were presented orally at the workshop. This article documents the workshop and results and provides context on previously available and recently developed methods.
C1 [Park, Michael A.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
[Aftosmis, Michael J.] NASA, Ames Res Ctr, Appl Modeling & Simulat Branch, Moffett Field, CA 94035 USA.
[Campbell, Richard L.; Carter, Melissa B.; Bangert, Linda S.] NASA, Langley Res Ctr, Configurat Aerodynam Branch, Hampton, VA 23681 USA.
RP Park, MA (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
NR 72
TC 3
Z9 3
U1 0
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD MAY-JUN
PY 2014
VL 51
IS 3
BP 987
EP 1001
DI 10.2514/1.C032589
PG 15
WC Engineering, Aerospace
SC Engineering
GA AJ8UT
UT WOS:000337984100027
ER
PT J
AU Duan, HY
Xu, R
Li, JC
Yuan, YG
Wang, QX
Hadi, NI
AF Duan Huanyun
Xu Rui
Li Jianchang
Yuan Yage
Wang Qiuxia
Hadi, Nomana Intekhab
TI Analysis on sustainable development countermeasures and barriers of
rural household biogas in China (vol 5, 043116, 2013)
SO JOURNAL OF RENEWABLE AND SUSTAINABLE ENERGY
LA English
DT Correction
C1 [Duan Huanyun; Xu Rui; Li Jianchang; Yuan Yage; Wang Qiuxia] Yannan Normal Univ, Coll Energy & Environm Sci, Solar Energy Inst, Kunming 650092, Peoples R China.
[Hadi, Nomana Intekhab] NASA, Ames Res Ctr, SETI Inst Affiliat, Moffett Field, CA 94035 USA.
RP Duan, HY (reprint author), Yannan Normal Univ, Coll Energy & Environm Sci, Solar Energy Inst, Kunming 650092, Peoples R China.
EM duanhuanyun@gmail.com; ecowatch.xr@gmail.com; jclee94213@yahoo.com.cn;
yuanyage@sina.cn; 798606608@qq.com; nomana.i.hadi@gmail.com
NR 1
TC 0
Z9 0
U1 1
U2 11
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1941-7012
J9 J RENEW SUSTAIN ENER
JI J. Renew. Sustain. Energy
PD MAY
PY 2014
VL 6
IS 3
AR 039901
DI 10.1063/1.4880535
PG 1
WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Energy & Fuels
SC Science & Technology - Other Topics; Energy & Fuels
GA AJ9ZS
UT WOS:000338072800048
ER
PT J
AU Abdo, AA
Abeysekara, AU
Allen, BT
Aune, T
Barber, AS
Berley, D
Braun, J
Chen, C
Christopher, GE
DeYoung, T
Dingus, BL
Ellsworth, RW
Gonzalez, MM
Goodman, JA
Hays, E
Hoffman, CM
Huntemeyer, PH
Imran, A
Kolterman, BE
Linnemann, JT
McEnery, JE
Morgan, T
Mincer, AI
Nemethy, P
Pretz, J
Ryan, JM
Parkinson, PMS
Schneider, M
Shoup, A
Sinnis, G
Smith, AJ
Vasileiou, V
Walker, GP
Williams, DA
Yodh, GB
AF Abdo, A. A.
Abeysekara, A. U.
Allen, B. T.
Aune, T.
Barber, A. S.
Berley, D.
Braun, J.
Chen, C.
Christopher, G. E.
DeYoung, T.
Dingus, B. L.
Ellsworth, R. W.
Gonzalez, M. M.
Goodman, J. A.
Hays, E.
Hoffman, C. M.
Huentemeyer, P. H.
Imran, A.
Kolterman, B. E.
Linnemann, J. T.
McEnery, J. E.
Morgan, T.
Mincer, A. I.
Nemethy, P.
Pretz, J.
Ryan, J. M.
Parkinson, P. M. Saz
Schneider, M.
Shoup, A.
Sinnis, G.
Smith, A. J.
Vasileiou, V.
Walker, G. P.
Williams, D. A.
Yodh, G. B.
TI Milagro observations of potential TeV emitters
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Astroparticle physics; Pulsars; Galaxies; Active galactic nuclei;
Gamma-rays
ID CYGNUS REGION; SPECTRUM; MARKARIAN-421; DISCOVERY; EMISSION; AREA
AB This paper reports the results from three targeted searches of Milagro TeV sky maps: two extragalactic point source lists and one pulsar source list. The first extragalactic candidate list consists of 709 candidates selected from the Fermi-LAT 2FGL catalog. The second extragalactic candidate list contains 31 candidates selected from the TeVCat source catalog that have been detected by imaging atmospheric Cherenkov telescopes (IACTs). In both extragalactic candidate lists Mkn 421 was the only source detected by Milagro. This paper presents the Milagro TeV flux for Mkn 421 and flux limits for the brighter Fermi-LAT extragalactic sources and for all TeVCat candidates. The pulsar list extends a previously published Milagro targeted search for Galactic sources. With the 32 new gamma-ray pulsars identified in 2FGL, the number of pulsars that are studied by both Fermi-LAT and Milagro is increased to 52. In this sample, we find that the probability of Milagro detecting a TeV emission coincident with a pulsar increases with the GeV flux observed by the Fermi-LAT in the energy range from 0.1 GeV to 100 GeV. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Abdo, A. A.; Abeysekara, A. U.; Barber, A. S.; Linnemann, J. T.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Allen, B. T.; Chen, C.; Yodh, G. B.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Aune, T.; Parkinson, P. M. Saz; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Berley, D.; Braun, J.; Goodman, J. A.; Smith, A. J.; Vasileiou, V.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Christopher, G. E.; Kolterman, B. E.; Mincer, A. I.; Nemethy, P.] NYU, Dept Phys, New York, NY 10003 USA.
[DeYoung, T.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Dingus, B. L.; Hoffman, C. M.; Imran, A.; Pretz, J.; Sinnis, G.; Walker, G. P.] Los Alamos Natl Lab, Grp P 23, Los Alamos, NM 87545 USA.
[Ellsworth, R. W.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA.
[Gonzalez, M. M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Hays, E.; McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Huentemeyer, P. H.] Michigan Technol Univ, Dept Phys, Houghton, MI 49931 USA.
[Morgan, T.; Ryan, J. M.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Schneider, M.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Shoup, A.] Ohio State Univ, Lima, OH 45804 USA.
[Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
RP Abeysekara, AU (reprint author), Michigan State Univ, Dept Phys & Astron, BioMed Phys Sci Bldg, E Lansing, MI 48824 USA.
EM udaraabeysekara@yahoo.com
OI Mincer, Allen/0000-0002-6307-1418; Dingus, Brenda/0000-0001-8451-7450
NR 20
TC 1
Z9 1
U1 0
U2 3
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
EI 1873-2852
J9 ASTROPART PHYS
JI Astropart Phys.
PD MAY-JUN
PY 2014
VL 57-58
BP 16
EP 25
DI 10.1016/j.astropartphys.2014.03.001
PG 10
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AJ4MY
UT WOS:000337651700004
ER
PT J
AU Golding, J
Steer, CD
Lowery, T
Jones, R
Hibbeln, JR
AF Golding, Jean
Steer, Colin D.
Lowery, Tony
Jones, Robert
Hibbeln, Joseph R.
TI Fish Consumption and Blood Mercury Levels: Golding et al. Respond
SO ENVIRONMENTAL HEALTH PERSPECTIVES
LA English
DT Letter
ID UK TOTAL DIET
C1 [Golding, Jean; Steer, Colin D.] Univ Bristol, Ctr Child & Adolescent Hlth, Bristol, RI 02809 USA.
[Lowery, Tony] Natl Ocean & Atmospher Adm, Natl Marine Fisheries Serv, Natl Seafood Inspect Lab, Pascagoula, MS USA.
[Jones, Robert] Ctr Dis Control & Prevent, Inorgan & Radiat Analyt Toxicol Branch, Atlanta, GA USA.
[Hibbeln, Joseph R.] NIAAA, NIH, Dept Hlth & Human Serv, Bethesda, MD USA.
RP Golding, J (reprint author), Univ Bristol, Ctr Child & Adolescent Hlth, Bristol, RI 02809 USA.
EM Jean.Golding@bristol.ac.uk
OI Golding, Jean/0000-0003-2826-3307
NR 3
TC 0
Z9 0
U1 0
U2 10
PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE
PI RES TRIANGLE PK
PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233,
RES TRIANGLE PK, NC 27709-2233 USA
SN 0091-6765
EI 1552-9924
J9 ENVIRON HEALTH PERSP
JI Environ. Health Perspect.
PD MAY
PY 2014
VL 122
IS 5
BP A120
EP A121
DI 10.1289/ehp.1307997R
PG 2
WC Environmental Sciences; Public, Environmental & Occupational Health;
Toxicology
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Toxicology
GA AJ3ZC
UT WOS:000337606300004
PM 24787643
ER
PT J
AU Nichols, JE
Isles, PDF
Peteet, DM
AF Nichols, Jonathan E.
Isles, Peter D. F.
Peteet, Dorothy M.
TI A novel framework for quantifying past methane recycling by
Sphagnum-methanotroph symbiosis using carbon and hydrogen isotope ratios
of leaf wax biomarkers
SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS
LA English
DT Article
ID N-ALKANE DISTRIBUTIONS; DELTA-D VALUES; ATMOSPHERIC CH4 GRADIENT;
NORTHERN PEATLAND; TESTATE AMEBAS; PLANTS; RECORD; HOLOCENE; BOG;
PHOTOSYNTHESIS
AB The concentration of atmospheric methane is strongly linked to variations in Earth's climate. Currently, we can directly reconstruct the total atmospheric concentration of methane, but not individual terms of the methane cycle. Northern wetlands, dominated by Sphagnum, are an important contributor of atmospheric methane, and we seek to understand the methane cycle in these systems. We present a novel method for quantifying the proportion of carbon Sphagnum assimilates from its methanotrophic symbionts using stable isotope ratios of leaf-wax biomarkers. Carbon isotope ratios of Sphagnum compounds are determined by two competing influences, water content and the isotope ratio of source carbon. We disentangled these effects using a combined hydrogen and carbon isotope approach. We constrained Sphagnum water content using the contrast between the hydrogen isotope ratios of Sphagnum and vascular plant biomarkers. We then used Sphagnum water content to calculate the carbon isotope ratio of Sphagnum's carbon pool. Using a mass balance equation, we calculated the proportion of recycled methane contributed to the Sphagnum carbon pool, "PRM." We quantified PRM in peat monoliths from three microhabitats in the Mer Bleue peatland complex. Modern studies have shown that water table depth and vegetation have strong influences on the peatland methane cycle on instrumental time scales. With this new approach, delta C-13 of Sphagnum compounds are now a useful tool for investigating the relationships among hydrology, vegetation, and methanotrophy in Sphagnum peatlands over the time scales of entire peatland sediment records, vital to our understanding of the global carbon cycle through the Late Glacial and Holocene.
C1 [Nichols, Jonathan E.; Peteet, Dorothy M.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Isles, Peter D. F.] Univ Vermont, Rubenstein Sch Environm & Nat Resources, Burlington, VT USA.
[Peteet, Dorothy M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Nichols, JE (reprint author), Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
EM jnichols@ldeo.columbia.edu
OI Nichols, Jonathan/0000-0003-3913-2206
FU National Science Foundation [ARC-1022979]; NASA Postdoctoral Program
FX The authors would like to thank Tim Moore and Nigel Roulet for
assistance in sample collection and for sharing methane flux data, Carl
Johnson for assistance with carbon isotope ratio measurements, and
Francesca McInerney and an anonymous reviewer for their helpful
comments. This research is supported by the National Science Foundation,
ARC-1022979. For part of this research, J. Nichols was supported by the
NASA Postdoctoral Program.
NR 45
TC 0
Z9 0
U1 1
U2 16
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1525-2027
J9 GEOCHEM GEOPHY GEOSY
JI Geochem. Geophys. Geosyst.
PD MAY
PY 2014
VL 15
IS 5
BP 1827
EP 1836
DI 10.1002/2014GC005242
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AJ4EQ
UT WOS:000337625100009
ER
PT J
AU Cabrol, NA
Herkenhoff, K
Knoll, AH
Farmer, J
Arvidson, R
Grin, E
Li, RX
Fenton, L
Cohen, B
Bell, JF
Yingst, RA
AF Cabrol, Nathalie A.
Herkenhoff, Kenneth
Knoll, Andrew H.
Farmer, Jack
Arvidson, Raymond
Grin, Edmond
Li, Ronxing
Fenton, Lori
Cohen, Barbara
Bell, James F., III
Yingst, R. Aileen
TI Sands at Gusev Crater, Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars; Gusev; Spirit; Sand; Texture; Sedimentology
ID GRAIN-SIZE DISTRIBUTIONS; SEDIMENT TREND ANALYSIS; SPIRIT ROVER;
IMAGE-ANALYSIS; PARTICLE-SIZE; MAADIM-VALLIS; ROCKS; EXPLORATION;
PARAMETERS; IDENTIFICATION
AB Processes, environments, and the energy associated with the transport and deposition of sand at Gusev Crater are characterized at the microscopic scale through the comparison of statistical moments for particle size and shape distributions. Bivariate and factor analyses define distinct textural groups at 51 sites along the traverse completed by the Spirit rover as it crossed the plains and went into the Columbia Hills. Fine-to-medium sand is ubiquitous in ripples and wind drifts. Most distributions show excess fine material, consistent with a predominance of wind erosion over the last 3.8 billion years. Negative skewness at West Valley is explained by the removal of fine sand during active erosion, or alternatively, by excess accumulation of coarse sand from a local source. The coarse to very coarse sand particles of ripple armors in the basaltic plains have a unique combination of size and shape. Their distribution display significant changes in their statistical moments within the similar to 400 m that separate the Columbia Memorial Station from Bonneville Crater. Results are consistent with aeolian and/or impact deposition, while the elongated and rounded shape of the grains forming the ripples, as well as their direction of origin, could point to Ma'adim Vallis as a possible source. For smaller particles on the traverse, our findings confirm that aeolian processes have dominated over impact and other processes to produce sands with the observed size and shape patterns across a spectrum of geologic (e.g., ripples and plains soils) and aerographic settings (e.g., wind shadows).
C1 [Cabrol, Nathalie A.; Grin, Edmond; Fenton, Lori] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
[Cabrol, Nathalie A.; Grin, Edmond] NASA Ames Res Ctr, Div Space Sci, Moffett Field, CA USA.
[Herkenhoff, Kenneth] US Geol Survey Astrogeol Team, Flagstaff, AZ USA.
[Knoll, Andrew H.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Farmer, Jack; Bell, James F., III] Arizona State Univ, Sch Earth & Planetary Explorat, Tempe, AZ USA.
[Arvidson, Raymond] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Li, Ronxing] Ohio State Univ, CEGE, Mapping & GIS Lab, Columbus, OH 43210 USA.
[Cohen, Barbara] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Yingst, R. Aileen] Planetary Sci Inst, Tucson, AZ USA.
RP Cabrol, NA (reprint author), Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
EM Nathalie.A.Cabrol@nasa.gov
FU National Aeronautics and Space Administration Mars Exploration Rover
mission
FX This work was performed for the Jet Propulsion Laboratory, California
Institute of Technology, sponsored by the National Aeronautics and Space
Administration Mars Exploration Rover mission. The authors want to
especially thank Steve Ostrowski (GIS & Mapping Lab Undergraduate
Research Assistant, The Ohio State University) for generating the map of
Spirit's traverse used in Figure 6. We are also extremely thankful to
Robert Craddock and an anonymous reviewer for their thorough reviews and
constructive remarks and suggestions.
NR 141
TC 2
Z9 2
U1 3
U2 13
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 MAY
PY 2014
VL 119
IS 5
BP 941
EP 967
DI 10.1002/2013JE004535
PG 27
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AJ5AX
UT WOS:000337693900003
ER
PT J
AU Hathaway, DH
Upton, L
AF Hathaway, D. H.
Upton, L.
TI The solar meridional circulation and sunspot cycle variability
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Sunspot Cycle
ID MAGNETIC-FIELD; TORSIONAL OSCILLATION; FLUX TRANSPORT; FLOW; SUN;
ROTATION; SURFACE; HELIOSEISMOLOGY; PHOTOSPHERE; EVOLUTION
AB We have measured the meridional motions of the magnetic elements in the Sun's surface layers since 1996 and find systematic and substantial variations. In general the meridional flow speed is fast at cycle minima and slow at cycle maxima. We find that these systematic variations are characterized by a weakening of the meridional flow on the poleward sides of the active (sunspot) latitudes. This can be interpreted as an inflow toward the sunspot zones superimposed on a more general poleward meridional flow profile. We also find variations in the meridional flow which vary from cycle to cycle. The meridional flow was slower at both the minimum and maximum of cycle 23 compared to similar phases of cycles 21, 22, and 24. Models of the magnetic flux transport by a variable meridional flow suggest that it can significantly modulate the size and timing of the following sunspot cycle through its impact on the Sun's polar magnetic fields. We suggest that the meridional flow variations observed in cycle 23 contributed to the weak polar fields at the end of the cycle which then produced a weak cycle 24 and the extraordinary cycle 23/24 minimum.
C1 [Hathaway, D. H.] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Upton, L.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Upton, L.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
RP Hathaway, DH (reprint author), NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
EM david.hathaway@nasa.gov
FU NASA [NAG5-10483]
FX The authors were supported by a grant from the NASA Living with a Star
Program to Marshall Space Flight Center. The HMI data used are courtesy
of the NASA/SDO and the HMI science team. The SOHO/MDI project was
supported by NASA grant NAG5-10483 to Stanford University. SOHO is a
project of international cooperation between ESA and NASA.
NR 46
TC 5
Z9 5
U1 1
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 MAY
PY 2014
VL 119
IS 5
BP 3316
EP 3324
DI 10.1002/2013JA019432
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AJ4DS
UT WOS:000337622100008
ER
PT J
AU Elfritz, JG
Keesee, AM
Buzulukova, N
Fok, MC
Scime, EE
AF Elfritz, J. G.
Keesee, A. M.
Buzulukova, N.
Fok, M. -C.
Scime, E. E.
TI First results using TWINS-derived ion temperature boundary conditions in
CRCM
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE magnetosphere; simulation; temperature
ID INTERPLANETARY MAGNETIC-FIELD; CENTRAL PLASMA SHEET; SOLAR-WIND CONTROL;
RING CURRENT; EARTHS MAGNETOSPHERE; GEOMAGNETIC STORMS; CURRENT SYSTEMS;
MODEL; SUBSTORM; IMAGES
AB We have integrated dynamic, spatiotemporally resolved ion temperature boundary conditions into the Comprehensive Ring Current Model (CRCM), which are based on 2-D equatorial maps derived from the Two Wide-Angle Imaging Neutral-Atom Spectrometers (TWINS) energetic neutral atom (ENA) data. The high-speed stream-driven event on 22 July 2009 is simulated and compared against an identical simulation using a statistically derived boundary condition model. ENA-derived temperatures allow users to include event-specific observations associated with a dynamic plasma sheet. This method also provides temperatures in the important region between geosynchronous orbit and the plasma sheet, a region which existing empirical models exclude. We find that the spatial and energy distributions of ring current flux and pressure have sensitive dependence on boundary conditions during this event. The coupling of boundary conditions to the time history of the convection field strength also plays an important role by throttling the influence of the boundary plasma on the inner magnetosphere. Simulated moments and spectra from our simulations are compared with remotely imaged ion temperatures from TWINS and also in situ energy spectra and temperature moments from Time History of Events and Macroscale Interactions during Substorms-D. Storm time dusk-dawn asymmetries consistent with observational data, such as Zhang et al. (2006), are reproduced well when CRCM is provided with the event-specific boundary model. A hot localized structure observed by TWINS at geosynchronous midnight during a strong northward interplanetary magnetic field interval is also reproduced with this boundary model, whereas the empirical boundary model fails to yield this feature.
C1 [Elfritz, J. G.; Keesee, A. M.; Scime, E. E.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
[Buzulukova, N.; Fok, M. -C.] NASA, Geospace Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Buzulukova, N.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Elfritz, JG (reprint author), W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
EM jelfritz@mix.wvu.edu
RI Keesee, Amy/J-8194-2014
OI Keesee, Amy/0000-0002-9719-3229
FU Southwest Research Institute, NSF [AGS- 1113478]; NASA EPSCoR
[NNX10AN08A]; NASA [NAS5-02099]
FX This work was carried out as a part of the TWINS NASA Explorer mission;
work at WVU was supported under subcontract to the Southwest Research
Institute, NSF grant AGS- 1113478 and NASA EPSCoR grant NNX10AN08A. The
authors would like to thank the members of the TWINS science team for
helpful discussions regarding the TWINS ENA data. The authors also
acknowledge the use of ACE solar wind data provided through Omni-Web. We
acknowledge NASA contract NAS5-02099 and V. Angelopoulos for use of data
from the THEMIS Mission. Specifically D. Larson and R. P. Lin for use of
SST data as well as C. W. Carlson and J. P. McFadden for use of ESA
data.
NR 55
TC 3
Z9 3
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 MAY
PY 2014
VL 119
IS 5
BP 3345
EP 3361
DI 10.1002/2013JA019555
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AJ4DS
UT WOS:000337622100011
ER
PT J
AU Connor, HK
Zesta, E
Ober, DM
Raeder, J
AF Connor, H. K.
Zesta, E.
Ober, D. M.
Raeder, J.
TI The relation between transpolar potential and reconnection rates during
sudden enhancement of solar wind dynamic pressure: OpenGGCM-CTIM results
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE MI coupling system; Magnetic reconnection; Cross Polar Cap Potential;
MHD modeling
ID IONOSPHERIC CONDUCTIVITY; MHD SIMULATIONS; AURORAL OVAL; JANUARY 10;
IMAGE FUV; POLAR; SATURATION; MAGNETOSPHERE; MAGNETOTAIL; MODEL
AB This study investigates how solar wind energy is deposited into the magnetosphere-ionosphere system during sudden enhancements of solar wind dynamic pressure (Psw), using the coupled Open Geospace General Circulation Model-Coupled Ionosphere Thermosphere Model (OpenGGCM-CTIM) 3-D global magnetosphere-ionosphere-thermosphere model. We simulate three unique events of solar wind pressure enhancements that occurred during negative, near-zero, and positive interplanetary magnetic field (IMF) Bz. Then, we examine the behavior of the dayside and nightside reconnection rates and quantify their respective contributions to cross polar cap potential (CPCP), a proxy of ionospheric plasma convection strength. The modeled CPCP increases after a Psw enhancement in all three cases, which agrees well with observations from the Defense Meteorological Satellite Program spacecraft and predictions from the assimilative mapping of ionospheric electrodynamics technique. In the OpenGGCM-CTIM model, dayside reconnection increases within 9-13min of the pressure impact, while nightside reconnection intensifies about 13-25min after the pressure increase. As the strong Psw compresses the dayside magnetosheath and, subsequently, the magnetotail, their magnetic fields intensify and activate stronger antiparallel reconnection on the dayside magnetopause first and near the central plasma sheet second. For southward IMF, dayside reconnection contributes to the CPCP enhancement 2-4 times more than nightside reconnection. For northward IMF, the dayside contribution weakens, and nightside reconnection contributes more to the CPCP enhancement. We find that high-latitude magnetopause reconnection during northward IMF produces sunward ionospheric plasma convection, which decreases the typical dawn-to-dusk ionosphere electric field. This results in a weaker dayside reconnection contribution to the CPCP during northward IMF.
C1 [Connor, H. K.] Univ New Mexico, Configurable Space Microsyst Innovat & Applicat, Albuquerque, NM 87131 USA.
[Zesta, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Connor, H. K.; Ober, D. M.] Air Force Res Lab, Kirtland AFB, NM USA.
[Raeder, J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
RP Connor, HK (reprint author), Univ New Mexico, Configurable Space Microsyst Innovat & Applicat, Albuquerque, NM 87131 USA.
EM hyunju.connor@cosmiac.org
FU Air Force Office of Scientific Research [11RV09COR]
FX The simulation data of this paper are available upon request. This work
was supported by a grant LBIR# 11RV09COR from the Air Force Office of
Scientific Research. We thank C. Y. Huang and Y.-J. Su for useful
discussions.
NR 50
TC 2
Z9 2
U1 3
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 MAY
PY 2014
VL 119
IS 5
BP 3411
EP 3429
DI 10.1002/2013JA019728
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AJ4DS
UT WOS:000337622100016
ER
PT J
AU Birn, J
Hesse, M
AF Birn, J.
Hesse, M.
TI The substorm current wedge: Further insights from MHD simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE substorm current wedge
ID MAGNETOTAIL; ASSOCIATION; FLOWS; FIELD
AB Using a recent magnetohydrodynamic simulation of magnetotail dynamics, we further investigate the buildup and evolution of the substorm current wedge (SCW), resulting from flow bursts generated by near-tail reconnection. Each flow burst generates an individual current wedge, which includes the reduction of cross-tail current and the diversion to region 1 (R1)-type field-aligned currents (earthward on the dawn and tailward on the duskside), connecting the tail with the ionosphere. Multiple flow bursts generate initially multiple SCW patterns, which at later times combine to a wider single SCW pattern. The standard SCW model is modified by the addition of several current loops, related to particular magnetic field changes: the increase of Bz in a local equatorial region (dipolarization), the decrease of |Bx|away from the equator (current disruption), and increases in |By|resulting from azimuthally deflected flows. The associated loop currents are found to be of similar magnitude, 0.1-0.3 MA. The combined effect requires the addition of region 2 (R2)-type currents closing in the near tail through dawnward currents but also connecting radially with the R1 currents. The current closure at the inner boundary, taken as a crude proxy of an idealized ionosphere, demonstrates westward currents as postulated in the original SCW picture as well as North-South currents connecting R1- and R2-type currents, which were larger than the westward currents by a factor of almost 2. However, this result should be applied with caution to the ionosphere because of our neglect of finite resistance and Hall effects.
C1 [Birn, J.] Space Sci Inst, Boulder, CO 80301 USA.
[Birn, J.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Birn, J (reprint author), Space Sci Inst, Boulder, CO 80301 USA.
EM jbirn@spacescience.org
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NASA [NNX13AD10G, NNX13AD21G]; NSF [1203711]
FX This work was performed mostly at Los Alamos National Laboratory under a
Guest Scientist agreement, supported by NASA grants NNX13AD10G and
NNX13AD21G and NSF grant 1203711. J.B. also acknowledges the hospitality
and support of the International Space Science Institute, Bern,
Switzerland, and fruitful discussions with Wolfgang Baumjohann and
members of the ISSI team on the substorm current wedge. Data necessary
to understand, evaluate, replicate, and build upon the reported research
will be made available upon request.
NR 23
TC 15
Z9 15
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 MAY
PY 2014
VL 119
IS 5
BP 3503
EP 3513
DI 10.1002/2014JA019863
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AJ4DS
UT WOS:000337622100022
ER
PT J
AU Birn, J
Runov, A
Hesse, M
AF Birn, J.
Runov, A.
Hesse, M.
TI Energetic electrons in dipolarization events: Spatial properties and
anisotropy
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE electron acceleration; dipolarization fronts; injections
ID TEST PARTICLE ORBITS; GEOSYNCHRONOUS OBSERVATIONS; MAGNETOTAIL;
ACCELERATION; SUBSTORMS; SIMULATIONS; INJECTIONS; TRANSPORT;
DISTRIBUTIONS; ENERGIZATION
AB Using the electromagnetic fields of an MHD simulation of magnetotail reconnection, flow bursts, and dipolarization, we further investigate the acceleration of electrons to suprathermal energies. Particular emphasis is on spatial properties and anisotropies as functions of energy and time. The simulation results are compared with Time History of Events and Macroscale Interactions during Substorms observations. The test particle approach successfully reproduces several observed injection features and puts them into a context of spatial maps of the injection region(s): a dominance of perpendicular anisotropies farther down the tail and closer to the equatorial plane, an increasing importance of parallel anisotropy closer to Earth and at higher latitudes, a drop in energy fluxes at energies below approximate to 10keV, coinciding with the plasma density drop, together with increases at higher energy, a triple peak structure of flux increases near 0 degrees, 90 degrees, and 180 degrees, and a tendency of flux increases to extend to higher energy closer to Earth and at lower latitudes. We identified the plasma sheet boundary layers and adjacent lobes as a main source region for both increased and decreased energetic electron fluxes, related to the different effects of adiabatic acceleration at high and low energies. The simulated anisotropies tend to exceed the observed ones, particularly for perpendicular fluxes at high energies. The most plausible reason is that the MHD simulation lacks the effects of anisotropy-driven microinstabilities and waves, which would reduce anisotropies.
C1 [Birn, J.] Space Sci Inst, Boulder, CO 80301 USA.
[Birn, J.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Runov, A.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA.
[Hesse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Birn, J (reprint author), Space Sci Inst, Boulder, CO 80301 USA.
EM jbirn@spacescience.org
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU U.S. Department of Energy; NASA [NNX13AD10G, NNX13AD21G, NAS5-0299,
NNX13AF81G]; NSF [1203711]; DLR [50 OC 0302]; International Space
Science Institute Bern, Switzerland
FX The simulation work was performed at Los Alamos under the auspices of
the U.S. Department of Energy, supported by NASA grants NNX13AD10G and
NNX13AD21G and NSF grant 1203711. THEMIS data analysis was supported by
NASA grants NAS5-0299 and NNX13AF81G. We thank V. Angelopoulos for use
of data from the THEMIS Mission, C. W. Carlson and J.P. McFadden for use
of ESA data, D. Larson and R. P. Lin for use of SST data, D. L. Turner
and P. Cruce for help with SST data calibration, and K.-H. Glassmeier,
U. Auster, and W. Baumjohann for the use of FGM data provided with
financial support through the DLR contract 50 OC 0302. We are grateful
to the hospitality and support by the International Space Science
Institute Bern, Switzerland, and the fruitful discussions with members
of the ISSI working group.
NR 37
TC 12
Z9 12
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAY
PY 2014
VL 119
IS 5
BP 3604
EP 3616
DI 10.1002/2013JA019738
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AJ4DS
UT WOS:000337622100029
ER
PT J
AU Nakano, S
Fok, MC
Brandt, PC
Higuchi, T
AF Nakano, S.
Fok, M-C.
Brandt, P. C.
Higuchi, T.
TI Estimation of temporal evolution of the helium plasmasphere based on a
sequence of IMAGE/EUV images
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE plasmasphere; electric field; data assimilation; magnetospheric
convection
ID 17 APRIL 2002; SQUARE-ROOT FILTERS; DATA ASSIMILATION; ELECTRIC-FIELD;
INNER MAGNETOSPHERE; KALMAN SMOOTHER; CLUSTER DATA; RING CURRENT;
ENSEMBLE; DYNAMICS
AB We have developed a technique for estimating the temporal evolution of the plasmaspheric helium ion density based on a sequence of extreme ultraviolet (EUV) data obtained from the IMAGE satellite. In the proposed technique, the estimation is obtained by incorporating EUV images from IMAGE into a two-dimensional fluid model of the plasmasphere using a data assimilation approach based on the ensemble transform Kalman filter. Since the motion and the spatial structure of the helium plasmasphere is strongly controlled by the electric field in the inner magnetosphere, the electric field around the plasmapause can also be estimated using the ensemble transform Kalman filter. We performed an experiment using synthetic images that were generated from the same numerical model under a certain condition. It was confirmed that the condition that generated the synthetic images was successfully reproduced. We also present some results obtained using real EUV imaging data. Finally, we discuss the possibility of estimating the density profile along a magnetic field line. Since each EUV image was taken from a different direction due to the motion of the IMAGE satellite, we could obtain the information on the density profile along a field line by combining multiple images.
C1 [Nakano, S.; Higuchi, T.] Res Org Informat & Syst, Inst Stat Math, Tachikawa, Tokyo, Japan.
[Nakano, S.; Higuchi, T.] Grad Univ Adv Studies, Sch Multidisciplinary Sci, Hayama, Kanagawa, Japan.
[Nakano, S.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Fok, M-C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Brandt, P. C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Nakano, S (reprint author), Res Org Informat & Syst, Inst Stat Math, Tachikawa, Tokyo, Japan.
EM shiny@ism.ac.jp
RI Brandt, Pontus/N-1218-2016;
OI Brandt, Pontus/0000-0002-4644-0306; Nakano, Shin'ya/0000-0003-0772-4610
FU Japan Society for the Promotion of Science [24740334]; Young Researcher
Overseas Visit Program of the Graduate University for Advanced Studies
FX The authors would like to thank B. R. Sandel and the University of
Arizona for providing the IMAGE/EUV data. The SOHO/SEM data were
provided by the Space Science Center of University of Southern
California. The authors would also like to thank N. Ness and the ACE
Science Center for providing the ACE data. The SYM-H and Dst indices
were provided by the World Data Center for Geomagnetism, Kyoto
University. The present study was supported by the Japan Society for the
Promotion of Science through a Grant-in-Aid for Young Scientists (B),
24740334, and was partially supported by Young Researcher Overseas Visit
Program of the Graduate University for Advanced Studies.
NR 48
TC 2
Z9 2
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAY
PY 2014
VL 119
IS 5
BP 3708
EP 3723
DI 10.1002/2013JA019734
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AJ4DS
UT WOS:000337622100035
ER
PT J
AU Nakano, S
Fok, MC
Brandt, PC
Higuchi, T
AF Nakano, S.
Fok, M. -C.
Brandt, P. C.
Higuchi, T.
TI Estimation of the helium ion density distribution in the plasmasphere
based on a single IMAGE/EUV image
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE plasmasphere; inner magnetosphere; inverse problem; magnetospheric
convection
ID 17 APRIL 2002; ELECTRON-DENSITY; RING CURRENT; PLASMAPAUSE; MODEL;
MAGNETOSPHERE
AB We have developed a technique by which to estimate the spatial distribution of plasmaspheric helium ions based on extreme ultraviolet (EUV) data obtained from the IMAGE satellite. The estimation is performed using a linear inversion method based on the Bayesian approach. The global imaging data from the IMAGE satellite enable us to estimate a global two-dimensional distribution of the helium ions in the plasmasphere. We applied this technique to a synthetic EUV image generated from a numerical model. This technique was confirmed to successfully reproduce the helium ion density that generated the synthetic EUV data. We also demonstrate how the proposed technique works for real data using two real EUV images.
C1 [Nakano, S.; Higuchi, T.] Res Org Informat & Syst, Inst Stat Math, Tachikawa, Tokyo, Japan.
[Nakano, S.; Higuchi, T.] Grad Univ Adv Studies, Sch Multidisciplinary Sci, Hayama, Kanagawa, Japan.
[Nakano, S.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Fok, M. -C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Brandt, P. C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Nakano, S (reprint author), Res Org Informat & Syst, Inst Stat Math, Tachikawa, Tokyo, Japan.
EM shiny@ism.ac.jp
RI Brandt, Pontus/N-1218-2016;
OI Brandt, Pontus/0000-0002-4644-0306; Nakano, Shin'ya/0000-0003-0772-4610
FU Japan Society for the Promotion of Science [24740334]
FX The authors would like to thank B. R. Sandel and the University of
Arizona for providing the IMAGE/EUV data. The SOHO/SEM data were
provided by the Space Science Center of the University of Southern
California. The SYM-H and Dst indices were provided by the World Data
Center for Geomagnetism, Kyoto University. This research was supported
by the Japan Society for the Promotion of Science through a Grant-in-Aid
for Young Scientists (B), 24740334.
NR 30
TC 1
Z9 1
U1 2
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 MAY
PY 2014
VL 119
IS 5
BP 3724
EP 3740
DI 10.1002/2013JA019733
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AJ4DS
UT WOS:000337622100036
ER
PT J
AU Edquist, KT
Korzun, AM
Dyakonov, AA
Studak, JW
Kipp, DM
Dupzyk, IC
AF Edquist, Karl T.
Korzun, Ashley M.
Dyakonov, Artem A.
Studak, Joseph W.
Kipp, Devin M.
Dupzyk, Ian C.
TI Development of Supersonic Retropropulsion for Future Mars Entry,
Descent, and Landing Systems
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID PERFORMANCE
AB Recent studies have concluded that Viking-era entry system deceleration technologies are extremely difficult to scale for progressively larger payloads (tens of metric tons) required for human Mars exploration. Supersonic retropropulsion is one of a few developing technologies that may enable future human-scale Mars entry systems. However, in order to be considered as a viable technology for future missions, supersonic retropropulsion will require significant maturation beyond its current state. This paper proposes major milestones for advancing the component technologies of supersonic retropropulsion such that it can be reliably used on Mars technology demonstration missions to land larger payloads than are currently possible using Viking-based systems. The development roadmap includes technology gates that are achieved through ground-based testing and high-fidelity analysis, culminating with subscale flight testing in Earth's atmosphere that demonstrates stable and controlled flight. The component technologies requiring advancement include large engines (100s of kilonewtons of thrust) capable of throttling and gimbaling, entry vehicle aerodynamics and aerothermodynamics modeling, entry vehicle stability and control methods, reference vehicle systems engineering and analyses, and high-fidelity models for entry trajectory simulations. Finally, a notional schedule is proposed for advancing the technology from suborbital free-flight tests at Earth through larger and more complex system-level technology demonstrations and precursor missions at Mars.
C1 [Edquist, Karl T.; Korzun, Ashley M.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
[Dyakonov, Artem A.] Blue Origin LLC, Kent, WA 98032 USA.
[Studak, Joseph W.] NASA, Lyndon B Johnson Space Ctr, Prop Syst Branch, Houston, TX 77058 USA.
[Kipp, Devin M.] CALTECH, Jet Prop Lab, Entry Descent & Landing Syst & Adv Technol Grp, Pasadena, CA 91109 USA.
[Dupzyk, Ian C.] Lunexa LLC, San Francisco, CA 94105 USA.
RP Edquist, KT (reprint author), NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, MS 489, Hampton, VA 23681 USA.
EM Karl.T.Exiquist@nasa.gov
FU Exploration Technology Development and Demonstration Program; NASA Ames
Research Center; NASA Johnson Space Center; Jet Propulsion Laboratory
FX The authors would like to acknowledge the support of the Exploration
Technology Development and Demonstration Program, which was managed at
NASA John H. Glenn Research Center at Lewis Field. The work documented
herein was performed as part of the program's Entry, Descent, and
Landing Technology Development Project, which was managed at NASA
Langley Research Center and supported by NASA Ames Research Center, NASA
Johnson Space Center, and the Jet Propulsion Laboratory. The authors
also wish to acknowledge the support of the Entry, Descent, and Landing
Systems Analysis team. Finally, the authors wish to acknowledge the
valuable contributions of Jeremy Shidner from Analytical Mechanics
Associates, Inc., in Hampton, Virginia; Ravi Prakash from the Jet
Propulsion Laboratory, California Institute of Technology in Pasadena,
California; and Kerry Zarchi from the NASA Ames Research Center in
Mountain View, California.
NR 28
TC 3
Z9 4
U1 0
U2 8
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 MAY-JUN
PY 2014
VL 51
IS 3
BP 650
EP 663
DI 10.2514/1.A32715
PG 14
WC Engineering, Aerospace
SC Engineering
GA AJ2NV
UT WOS:000337495500002
ER
PT J
AU Berry, SA
Rhode, MN
Edquist, K
AF Berry, Scott A.
Rhode, Matthew N.
Edquist, Karl
TI Supersonic Retropropulsion Validation Experiment in the NASA Langley
Unitary Plan Wind Tunnel
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID COMPUTATIONAL FLUID-DYNAMICS; MARS ENTRY; DESCENT
AB The development of supersonic retropropulsion, an enabling technology for heavy payload exploration missions to Mars, is the focus of the present paper. A new experimental model, intended to provide computational fluid dynamics model validation data, was recently designed for the Langley Research Center Unitary Plan Wind Tunnel test section 2. Pretest analyses using modern computational fluid and thermal analysis tools were instrumental for sizing., and refining the model, over the Mach number range of 2.4-4.6, such that tunnel blockage and internal flow separation issues would be minimized. A 5-in.-diam 70 deg sphere-cone forebody, which accommodates up to four 4 : 1 area ratio nozzles, followed by a 9.55-in.-long cylindrical aftbody, was developed for this study based on the computational results. The model was designed to allow for a large number of surface pressure measurements on the forebody and aftbody. Supplemental data included high-speed schlieren video and internal pressures and temperatures. The run matrix was developed to allow for the quantification of various sources of experimental uncertainty, such as random errors due to run-to-run variations and bias errors due to flowfield or model misalignments Observations and trends from this initial test in the Unitary Plan Wind Tunnel are presented.
C1 [Berry, Scott A.; Rhode, Matthew N.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
[Edquist, Karl] NASA, Langley Res Ctr, Atmospher Hight & Entry Syst Branch, Hampton, VA 23681 USA.
RP Berry, SA (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, M-S 408A, Hampton, VA 23681 USA.
FU NASA's Exploration Technology Development and Demonstration (ETDD)
Program; NASA's Fundamental Aeronautics Program (FAP); ETDD's Entry,
Descent, and Landing Technology Development Project; FAP's Hypersonics
Project
FX The authors would like to acknowledge the support of NASA's Exploration
Technology Development and Demonstration (ETDD) Program and Fundamental
Aeronautics Program (FAP). ETDD's Entry, Descent, and Landing Technology
Development Project and FAP's Hypersonics Project, both managed at NASA
Langley Research Center, supported the work documented herein.
Furthermore, the following individuals were instrumental in this
experimental endeavor: Chris Laws, Courtney Spells, Andrew McCrea, Bil
Kleb, Guy Schauerhamer, Kerry Trumble, Bill Oberkampf, Ashley Korzun,
Ruth Amundsen, Aaron Fuchs, Bryan Falman, Ricky Hall, Paul Bagby, and
Steve Jones.
NR 24
TC 4
Z9 4
U1 2
U2 5
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 MAY-JUN
PY 2014
VL 51
IS 3
BP 664
EP 679
DI 10.2514/1.A32649
PG 16
WC Engineering, Aerospace
SC Engineering
GA AJ2NV
UT WOS:000337495500003
ER
PT J
AU Zarchi, KA
Schauerhamert, DG
Kleb, WL
Carlson, JR
Edquist, KT
AF Zarchi, Kerry A.
Schauerhamert, Daniel G.
Kleb, William L.
Carlson, Jan-Renee
Edquist, Karl T.
TI Analysis of Navier-Stokes Codes Applied to Supersonic Retropropulsion
Wind-Tunnel Test
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID MARS ENTRY; DESCENT
AB Advancement of supersonic retropropulsion as a technology will rely heavily on the ability of computational methods to accurately predict vehicle aerodynamics during atmospheric descent, where supersonic retropropulsion will be employed. A wind-tunnel test at the NASA Langley Unitary Plan Wind Tunnel was specifically designed to aid in the support of Navier-Stokes codes for supersonic retropropulsion applications. Three computational fluid dynamics codes [data parallel line relaxation, fully unstructured Navier-Stokes three-dimensional, and overset grid flow solver] were exercised for multiple nozzle configurations for a range of freestream Mach numbers and nozzle thrust coefficients. The computational fluid dynamics pretest analysis of this wind-tunnel test aided in the test model design process by identifying the potential for tunnel blockage or unstart, of liquefaction within the plume, and of separation occurring at the internal fingers of the nozzles. This analysis led to a reduced model diameter, heating of the plenum, and reducing the nozzle area ratio, and the requirement to radius the corners at the fingers, to counter these potentials, respectively. Comparisons to test data were used to determine the existing capability of the codes to accurately model this complex flow, identify modeling shortcomings, and gain insight into the computational requirements necessary for correctly computing these flows. All three codes predict similar surface pressure coefficients and flowfield structures, such as jet termination shock, interface, bow shocks, and recirculation regions. However, the codes differ on the level of unsteadiness predicted.
C1 [Zarchi, Kerry A.] NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA.
[Schauerhamert, Daniel G.] Jacobs Technol Inc, Appl Aerosci & Computat Fluid Dynam Branch, Houston, TX 77058 USA.
[Kleb, William L.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
[Carlson, Jan-Renee] NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA.
[Edquist, Karl T.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
RP Zarchi, KA (reprint author), NASA, Ames Res Ctr, Aerothermodynam Branch, Mail Stop 230-2, Moffett Field, CA 94035 USA.
NR 37
TC 3
Z9 3
U1 1
U2 4
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAY-JUN
PY 2014
VL 51
IS 3
BP 680
EP 692
DI 10.2514/1.A32744
PG 13
WC Engineering, Aerospace
SC Engineering
GA AJ2NV
UT WOS:000337495500004
ER
PT J
AU Schauerhamer, DG
Zarchi, KA
Kleb, WL
Carlson, JR
Edquist, KT
AF Schauerhamer, Daniel Guy
Zarchi, Kerry A.
Kleb, William L.
Carlson, Jan-Renee
Edquist, Karl. T.
TI Supersonic Retropropulsion Computational Fluid Dynamics Validation with
Langley 4 x 4 Foot Test Data
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID UNSTRUCTURED GRIDS; TURBULENT FLOWS; MARS ENTRY; DESCENT
AB Validation of computational fluid dynamics for supersonic retropropulsion is shown through the comparison of three Navier-Stokes solvers and wind-tunnel test results. The test was designed specifically for computational fluid dynamics validation and was conducted in the NASA Langley Research Center supersonic 4 x 4 foot Unitary Plan Wind Tunnel. The test includes variations in the number of nozzles, Mach and Reynolds numbers, thrust coefficient, and angles of orientation. Code-to-code and code-to-test comparisons are encouraging, and possible error sources are discussed.
C1 [Schauerhamer, Daniel Guy] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Zarchi, Kerry A.] NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA.
[Kleb, William L.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
[Carlson, Jan-Renee] NASA, Langley Res Ctr, Computat Aerosci Branch, Hampton, VA 23681 USA.
[Edquist, Karl. T.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
RP Schauerhamer, DG (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
FU Exploration Technology Development and Demonstration (ETDD) Program;
NASA Ames Research Center; NASA Johnson Space Center; Jet Propulsion
Laboratory
FX Pieter G. Buning of NASA Langley Research Center, Hampton, Virginia;
Phillip C. Stuart and Darby J. Vicker of NASA Johnson Space Center,
Houston, Texas; and Thomas M. Booth of Jacobs Technology, Houston,
Texas, provided valuable guidance on gridding and solver best practices
for OVERFLOW. William T. Jones of NASA Langley Research Center, Hampton,
Virginia, provided the GridEx/batchEx unstructured grid generation
framework and helped with its application to generate FUN3D grids. Todd
R. White and Andrew J. Hyatt of ERC Inc., Moffett Field, California,
helped develop DPLR best practices and provided overset gridding
assistance for DPLR cases. David A. Saunders of ERC Inc., Moffett Field,
California, developed the code used for OVERFLOW and DPLR simulated
Schlieren/shadowgraph visualizations. The authors would like to
acknowledge the support of the Exploration Technology Development and
Demonstration (ETDD) Program, which was managed at NASA Glenn Research
Center. The work documented herein was performed as part of ETDD's
Entry, Descent, and Landing Technology Development Project, which was
managed at NASA Langley Research Center and supported by NASA Ames
Research Center, NASA Johnson Space Center, and the Jet Propulsion
Laboratory.
NR 32
TC 3
Z9 3
U1 0
U2 1
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 MAY-JUN
PY 2014
VL 51
IS 3
BP 693
EP 714
DI 10.2514/1.A32693
PG 22
WC Engineering, Aerospace
SC Engineering
GA AJ2NV
UT WOS:000337495500005
ER
PT J
AU Codoni, JR
Berry, SA
AF Codoni, Joshua R.
Berry, Scott A.
TI Supersonic Retropropulsion Dynamic Data Analysis from NASA Langley
Unitary Plan Wind Tunnel
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID ENTRY
AB A supersonic retropropulsion experiment was recently conducted at NASA Langley Research Center's Unitary Plan Wind Tunnel, test section 2, for a range of Mach numbers from 2.4 to 4.6. A 5-in.-diam 70 deg sphere-cone forebody with a 9.55 in. cylindrical aftbody section was the experimental model used, which is capable of multiple retrorocket configurations. These configurations include a single central nozzle on the center point of the forebody, three nozzles at the forebody half-radius, and a combination of the first two configurations. A series of measurements were achieved through various instrumentation, including forebody and aftbody surface pressures, internal pressures and temperatures, and high-speed schlieren visualization. Several high-speed pressure transducers on the forebody and in the plenum were implemented to look at unsteady flow effects. The following work focuses on analyzing frequency traits due to the unsteady flow for a range of thrust coefficients for single-, tri-, and quadnozzle test cases at a freestream Mach number of 4.6 and an angle of attack ranging from 0 to +20 deg. This analysis uses MATLAB (R)'s fast Fourier transform, Welch's method (modified average of a periodogram), to create a power spectral density and analyze any high-speed pressure transducer frequency traits due to the unsteady flow.
C1 [Codoni, Joshua R.] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22903 USA.
[Berry, Scott A.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
RP Codoni, JR (reprint author), Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22903 USA.
NR 19
TC 0
Z9 0
U1 2
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAY-JUN
PY 2014
VL 51
IS 3
BP 715
EP 723
DI 10.2514/1.A32619
PG 9
WC Engineering, Aerospace
SC Engineering
GA AJ2NV
UT WOS:000337495500006
ER
PT J
AU Berry, SA
Rhode, MN
Edquist, KT
AF Berry, Scott A.
Rhode, Matthew N.
Edquist, Karl T.
TI Supersonic Retropropulsion Experimental Results from NASA Ames 9 x 7
Foot Supersonic Wind Tunnel
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID FOURIER-TRANSFORM; MARS ENTRY; DESCENT
AB Supersonic retropropulsion was experimentally examined in the Ames Research Center 9 x 7 Foot Supersonic Wind Tunnel at Mach 1.8 and 2.4. The model, previously designed for and tested in the Langley Research Center Unitary Plan Wind Tunnel at Mach 2.4, 3.5, and 4.6, was a 5-in.-diam 70 deg sphere-cone forebody with a 9.55-in.-long cylindrical aftbody. The forebody was designed to accommodate up to four 4:1 area ratio nozzles, one on the model centerline and the other three on the half-radius spaced 120 deg apart. Surface pressure and flow visualization were the primary measurements, including high-speed data to investigate the dynamics of the interactions between the bow and nozzle shocks. Three blowing configurations were tested with thrust coefficients up to 10 and angles of attack up to 20 deg. Results and observations from the test are provided.
C1 [Berry, Scott A.; Rhode, Matthew N.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
[Edquist, Karl T.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
RP Berry, SA (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, Mail Stop 408a, Hampton, VA 23681 USA.
FU NASA's Exploration Technology Development and Demonstration (ETDD)
Program; NASA's Fundamental Aeronautics Program (FAP)
FX The authors would like to acknowledge the support of NASA's Exploration
Technology Development and Demonstration (ETDD) Program and Fundamental
Aeronautics Program (FAP). The work documented herein was performed
jointly by both ETDD's Entry, Descent, and Landing Technology
Development Project and FAP's Hypersonics Project, both managed at NASA
Langley Research Center. Furthermore, the following individuals were
instrumental to this experimental effort: Joe Giuliana, Paul Tucker,
Kerry Trumble, Artem Dyakonov, Josh Codoni, Chris Cordell, Guy
Schauerhamer, Ashley Korzun, Jennifer Everett, Max Amaya, Tom Bridge,
James Brown, Bill Browning, Jay Carolino, Maureen Delgado, Joel Hoffman,
John Holmberg, Rudy Jaklitsch, Matt Krakenburg, David Lam, Pam Pfohl,
Scott Richey, Tom Romer, Nestor Rostran, Art Silva, Robin Townsend, Dale
Tuttle, Jonathan VanHorn, Bill VanZuylen, and Tom Volden.
NR 24
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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 MAY-JUN
PY 2014
VL 51
IS 3
BP 724
EP 734
DI 10.2514/1.A32650
PG 11
WC Engineering, Aerospace
SC Engineering
GA AJ2NV
UT WOS:000337495500007
ER
PT J
AU Schauerhamer, DG
Zarchi, KA
Kleb, WL
Edquist, KT
AF Schauerhamer, Daniel Guy
Zarchi, Kerry A.
Kleb, William L.
Edquist, Karl T.
TI Supersonic Retropropulsion Computational-Fluid-Dynamics Validation with
Ames 9 x 7 Foot Test Data
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID UNSTRUCTURED GRIDS; TURBULENT FLOWS; MARS ENTRY; DESCENT
AB A validation study of computational fluid dynamics for supersonic retropropulsion was conducted using three Navier-Stokes flow solvers. The study compared results from the computational-fluid-dynamics codes to each other and to wind-tunnel test data obtained in the NASA Ames Research Center 9 x 7 ft Unitary Plan Wind Tunnel. Comparisons include surface pressure coefficient as well as unsteady plume effects and cover a range of Mach numbers, levels of thrust, and angles of orientation for zero-, one-, three-, and four-nozzle configurations. Flow-structure behavior changed with thrust and angle of orientation for all nozzle configurations. In general, the solvers compared best with the test data for the steadier cases of the one-nozzle and high-thrust three-nozzle configurations. Deviation in surface pressure was noted for the more unsteady cases and near transitions in behavioral modes. Strengths and weaknesses of the solvers are identified, and possible error sources are discussed.
C1 [Schauerhamer, Daniel Guy] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Zarchi, Kerry A.] NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA.
[Kleb, William L.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
[Edquist, Karl T.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
RP Schauerhamer, DG (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
FU Exploration Technology Development and Demonstration (ETDD) Program;
NASA Ames Research Center; NASA Johnson Space Center; Jet Propulsion
Laboratory
FX Pieter G. Burling of NASA Langley Research Center, Hampton, Virginia,
and Phillip C. Stuart, Thomas M. Booth, and Darby J. Vicker of NASA
Johnson Space Center, Houston, Texas provided valuable guidance on
gridding and solver best practices for OVERFLOW. William T. Jones of
NASA Langley Research Center, Hampton, Virginia, provided the
GridEx/batchEx unstructured grid-generation framework and helped with
its application to generate FUN3D grids. Todd R. White and Andrew J.
Hyatt of ERC Inc., Moffett Field, California, helped develop DPLR best
practices and provided overset gridding assistance for DPLR cases. David
A. Saunders of ERC Inc., Moffett Field, California, developed the code
used for OVERFLOW and DPLR simulated Schlieren/shadowgraph
visualizations. The authors would like to acknowledge the support of the
Exploration Technology Development and Demonstration (ETDD) Program,
which was managed at NASA Glenn Research Center. The work documented
herein was performed as part of ETDD's Entry, Descent, and Landing
Technology Development Project, which was managed at NASA Langley
Research Center and supported by NASA Ames Research Center, NASA Johnson
Space Center, and the Jet Propulsion Laboratory.
NR 22
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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 MAY-JUN
PY 2014
VL 51
IS 3
BP 735
EP 749
DI 10.2514/1.A32694
PG 15
WC Engineering, Aerospace
SC Engineering
GA AJ2NV
UT WOS:000337495500008
ER
PT J
AU Chen, YK
Gokcen, T
AF Chen, Yih-Kanq
Goekcen, Tahir
TI Implicit Coupling Approach for Simulation of Charring Carbon Ablators
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID THERMAL RESPONSE; SHAPE CHANGE; ABLATION; PROGRAM; MODEL
AB This study demonstrates that coupling of a material thermal response code and a flow solver with nonequilibrium gas surface interaction for simulation of charring carbon ablators can be performed using an implicit approach. The material thermal response code used in this study, is the three-dimensional version of fully implicit ablation and thermal response program, which predicts charring material thermal response and shape change on hypersonic space vehicles. The flow code solves the reacting Navier-Stokes equations using data-parallel line relaxation method. Coupling between the material response and flow codes is performed by solving the surface mass balance in the flow solver and the surface energy balance in the material response code. Thus, the material surface recession is predicted in the flow code, and the surface temperature and pyrolysis gas injection rate are computed in the material response code. It is demonstrated that the time-lagged explicit approach is sufficient for simulations at low surface heating conditions, in which the surface ablation rate is not a strong function of the surface temperature. At elevated surface heating conditions, the implicit approach has to be taken because the carbon ablation rate becomes a stiff function of the surface temperature, and thus the explicit approach appears to be inappropriate, resulting in severe numerical oscillations of predicted surface temperature. Implicit coupling for simulation of arc-jet models is performed, and the predictions are compared with measured data. Implicit coupling for trajectory-based simulation of Stardust forebody heat shield is also conducted. The predicted stagnation point total recession is compared with that predicted using the chemical equilibrium surface assumption.
C1 [Chen, Yih-Kanq] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
[Goekcen, Tahir] ERC Inc, Aerothermodynam Branch, 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.
FU NASA Fundamental Aeronautics Program under Hypersonics Entry,
Descending, and Landing (EDL) Project
FX This work is funded by the NASA Fundamental Aeronautics Program under
the Hypersonics Entry, Descending, and Landing (EDL) Project.
NR 24
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U1 0
U2 4
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD MAY-JUN
PY 2014
VL 51
IS 3
BP 779
EP 788
DI 10.2514/1.A32753
PG 10
WC Engineering, Aerospace
SC Engineering
GA AJ2NV
UT WOS:000337495500011
ER
PT J
AU Mazaheri, A
Bruce, WE
Mesick, NJ
Sutton, K
AF Mazaheri, Alireza
Bruce, Walter E., III
Mesick, Nathaniel J.
Sutton, Kenneth
TI Methodology for Flight-Relevant Arc-Jet Testing of Flexible Thermal
Protection Systems
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB A methodology to correlate flight aeroheating environments to the arc-jet environment is presented. For a desired hot-wall flight heating rate, the methodology provides the arc-jet bulk enthalpy for the corresponding cold-wall heating rate. A series of analyses were conducted to examine the effects of the test sample model holder geometry to the overall performance of the test sample. The analyses were compared with arc-jet test samples, and challenges and issues are presented. The transient flight environment was calculated for the Hypersonic Inflatable Aerodynamic Decelerator Earth Atmospheric Reentry Test vehicle, which is a planned demonstration vehicle using a large inflatable, flexible thermal protection system to reenter the Earth's atmosphere from the International Space Station. A series of correlations were developed to define the relevant arc-jet test environment to properly approximate the vehicle flight environment. The computed arc-jet environments were compared with the measured arc-jet values to define the uncertainty of the correlated environment. The results show that, for a given flight surface heat flux and a fully catalytic thermal protection system, the flight-relevant arc-jet heat flux increases with the arc-jet bulk enthalpy, while for a noncatalytic thermal protection system, the arc-jet heat flux decreases with the bulk enthalpy.
C1 [Mazaheri, Alireza] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
[Bruce, Walter E., III] NASA, Langley Res Ctr, Struct & Thermal Syst Branch, Hampton, VA 23681 USA.
[Mesick, Nathaniel J.] Sci Syst & Applicat Inc, Mech Syst Branch, Hampton, VA 23666 USA.
[Sutton, Kenneth] Natl Inst Aerosp, Aerothermodynam Branch, Hampton, VA 23666 USA.
RP Mazaheri, A (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, M-S 408A, Hampton, VA 23681 USA.
EM Ali.R.Mazatieri@nasa.gov
FU Hypersonic Inflatable Aerodynamic Decelerator (HIAD) project; HIAD Earth
Atmospheric Reentry Test project
FX The present work was supported by the Hypersonic Inflatable Aerodynamic
Decelerator (HIAD) and the HIAD Earth Atmospheric Reentry Test projects.
The authors would also like to thank John R. Simms and Matthew P.
Kardell at the Boeing Large Core Arc Tunnel facility who successfully
programmed the arc heater controller to match the arc-jet heat flux and
flight surface pressure from the presented correlations. Thanks also go
to the reviewers for their thorough review of the paper and constructive
comments.
NR 18
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U1 2
U2 7
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 MAY-JUN
PY 2014
VL 51
IS 3
BP 789
EP 800
DI 10.2514/1.A32721
PG 12
WC Engineering, Aerospace
SC Engineering
GA AJ2NV
UT WOS:000337495500012
ER
PT J
AU Palmer, G
Prabhu, D
Cruden, BA
AF Palmer, Grant
Prabhu, Dinesh
Cruden, Brett A.
TI Aeroheating Uncertainties in Uranus and Saturn Entries by the Monte
Carlo Method
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID TRANSPORT PROPERTY COMPUTATIONS; RECOMMENDED COLLISION INTEGRALS;
VIBRATIONAL-RELAXATION; VOYAGER MEASUREMENTS; ELASTIC-SCATTERING; HELIUM
ABUNDANCE; CHARGE-TRANSFER; HYDROGEN; MARS; HE
AB The 2013-2022 decadal survey ("Vision and Voyages for Planetary Science in the Decade 2013-2022," National Research Council Rept., National Academy Press, Washington, D.C., 2011) for planetary exploration has identified probe missions to Uranus and Saturn as high priorities. This work endeavors to examine the uncertainty for determining aeroheating in such entry environments. Representative entry trajectories are constructed using the TRAJ software. Flowfields at selected points on the trajectories are then computed using the data parallel line relaxation computational fluid dynamics code. A Monte Carlo study is performed on the data parallel line relaxation input parameters to determine the uncertainty in the predicted aeroheating, and correlation coefficients are examined to identify which input parameters show the most influence on the uncertainty. A review of the present best practices for input parameters (for example, transport coefficient and vibrational relaxation time) is also conducted. It is found that the 2 sigma-uncertainty for heating on the Uranus entry is no more than 2.1%, assuming an equilibrium catalytic wall, with the uncertainty being determined primarily by diffusion and an H-2 recombination rate within the boundary layer. However, if the wall is assumed to be partially catalytic or noncatalytic, this uncertainty may increase to as large as 18%. The catalytic wall model can contribute over three times the change in heat flux and a 20% variation in film coefficient. Therefore, coupled material response/fluid dynamic models are recommended for this problem. It was also found that much of this variability is artificially suppressed when a constant Schmidt number approach is implemented. Because the boundary layer is reacting, it is necessary to employ self-consistent effective binary diffusion to obtain a correct thermal transport solution. For Saturn entries, the 2 sigma uncertainty for convective heating was less than 3.7%. The major uncertainty driver was dependent on shock temperature/velocity, changing from boundary-layer thermal conductivity to diffusivity and then to shock-layer ionization rate as velocity increases. While radiative heating for Uranus entry was negligible, the nominal solution for Saturn computed up to 20% radiative heating at the highest velocity examined. The radiative heating followed a nonnormal distribution, with up to a three-time variation in magnitude. This uncertainty is driven by the H-2 dissociation rate, as H-2 that persists in the hot nonequilibrium zone contributes significantly to radiation.
C1 [Palmer, Grant; Prabhu, Dinesh; Cruden, Brett A.] ERC Inc, Moffett Field, CA 94035 USA.
RP Palmer, G (reprint author), NASA, Ames Res Ctr, Washington, DC 20546 USA.
FU NASA [NNA10DE12C]
FX The authors are supported by NASA contract NNA10DE12C to ERC, Inc. The
authors would like to thank Helen Hwang, Suman Muppidi, and Aaron
Brandis for useful discussions. Michael Barnhardt is acknowledged for
assistance with updating the data parallel line relaxation databases and
running test case comparisons.
NR 43
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U1 0
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 MAY-JUN
PY 2014
VL 51
IS 3
BP 801
EP 814
DI 10.2514/1.A32768
PG 14
WC Engineering, Aerospace
SC Engineering
GA AJ2NV
UT WOS:000337495500013
ER
PT J
AU Yang, HQ
Peugeot, J
AF Yang, H. Q.
Peugeot, John
TI Propellant Sloshing Parameter Extraction from
Computational-Fluid-Dynamics Analysis
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID BEHAVIOR
AB Propellant slosh is a potential source of disturbance critical to the stability of space vehicles. The sloshing dynamics are typically represented by a mechanical model of a spring-mass-damper system. This mechanical model is then included in the equation of motion of the entire vehicle for guidance, navigation and control analysis. The typical parameters required by the mechanical model include the natural frequency of the sloshing, sloshing mass, sloshing mass center coordinates, and critical damping coefficient. During the 1960s in the U.S. space program, these parameters were computed either from analytical solutions for simple geometries or by experimental testing for the subscale configurations. The purpose of this work is to demonstrate the soundness of a computational-fluid-dynamics approach in modeling the detailed fluid dynamics of tank sloshing and the excellent accuracy in extracting mechanical properties for different tank configurations and at different fill levels. As the first attempt, the work focuses mainly on the identification of the natural frequency and the equivalent slosh mass from the simulations. The paper presents verification against the analytical solution of natural frequency for two- and three-dimensional straight cylinders, and validation against experimental results for subscale Centaur Liquid Oxygen and Liquid Hydrogen tanks with and without baffles. The results show that computational-fluid-dynamics technology can provide accurate mechanical parameters for any tank configuration, and is especially valuable to the future design of propellant tanks.
C1 [Yang, H. Q.] CFD Res Corp, Huntsville, AL 35805 USA.
[Peugeot, John] NASA, George C Marshall Space Flight Ctr, Fluid Dynam Branch ER42, Huntsville, AL 35812 USA.
RP Yang, HQ (reprint author), CFD Res Corp, 215 Wynn Dr, Huntsville, AL 35805 USA.
EM hqy@cfdrc.com; John.W.Peugeot@nasa.gov
FU Jacobs Engineering NASA Marshall Space Flight Center (MSFC) Engineering,
Science, and Technical Services (ESTS) [NNM05AB50C]
FX This study was performed under a task order of the Jacobs Engineering
NASA Marshall Space Flight Center (MSFC) Engineering, Science, and
Technical Services (ESTS) contract NNM05AB50C. Ram Ramachandran was the
Jacobs ESTS Task Lead, and Jeff West (MSFC Fluid Dynamics Branch, ER42)
was the NASA MSFC Task Monitor.
NR 15
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Z9 0
U1 1
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 MAY-JUN
PY 2014
VL 51
IS 3
BP 908
EP 916
DI 10.2514/1.A32608
PG 9
WC Engineering, Aerospace
SC Engineering
GA AJ2NV
UT WOS:000337495500023
ER
PT J
AU Yang, YM
Komjathy, A
Langley, RB
Vergados, P
Butala, MD
Mannucci, AJ
AF Yang, Yu-Ming
Komjathy, Attila
Langley, Richard B.
Vergados, Panagiotis
Butala, Mark D.
Mannucci, Anthony J.
TI The 2013 Chelyabinsk meteor ionospheric impact studied using GPS
measurements
SO RADIO SCIENCE
LA English
DT Article
DE remote sensing; GPS; total electron content; ionospheric disturbance;
asteriod impact; natural hazards
AB On 15 February 2013, the Chelyabinsk meteor event (the largest in size since 1908) provided a unique opportunity to observe ionospheric perturbations associated with the ablation and ionospheric impact of the meteor using GPS measurements. The hypersonic bolide generated powerful shock waves while acoustic perturbations in the atmosphere led to the upward propagation of acoustic and gravity waves into the ionosphere. In our research, we applied two different techniques to detect ionospheric disturbances in dual-frequency global positioning system (GPS) measurements during the meteor impact event. The data were collected from near-field GPS networks in Russia, GPS Earth Observation Network (GEONET) in Japan, and Plate Boundary Observatory (PBO) stations in the coterminous U.S. Using a novel wavelet coherence detection technique, we were able to identify three different wave trains in the measurements collected from the nearest GPS station to the meteor impact site, with frequencies of approximately 4.0-7.8 mHz, 1.0 -2.5 mHz, and 2.7-11 mHz at 03:30 UTC. We estimated the speed and direction of arrival of the total electron content (TEC) disturbances by cross-correlating TEC time series for every pair of stations in several areas of the GEONET and PBO networks. The results may be characterized as three different types of traveling ionospheric disturbances (TIDs). First, the higher-frequency (4.0-7.8 mHz) disturbances were observed around the station ARTU in Arti, Russia (56.43 degrees N, 58.56 degrees E), with an estimated mean propagation speed of about 862 +/- 65m/s (with 95% confidence interval). Another type of TID disturbance related to the wave trains was identified in the lower frequency band (1.0-2.5 mHz), propagating with a mean speed of 362 +/- 23m/s. The lower frequency ionospheric perturbations were observed at distances of 300-1500km away from Chelyabinsk. The third type of TID wave train was identified using the PBO stations in the relative short-period range of 1.5-6min (2.7-11 mHz) with a mean propagation speed of 733 +/- 36m/s. The observed short-period ionospheric perturbations in the U.S. region is, to the best of our knowledge, the first observational evidence of the coincident the long-range meteor-generated infrasound signals propagating in the ionosphere.
C1 [Yang, Yu-Ming; Komjathy, Attila; Vergados, Panagiotis; Butala, Mark D.; Mannucci, Anthony J.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
[Komjathy, Attila; Langley, Richard B.] Univ New Brunswick, Dept Geodesy & Geomat Engn, Fredericton, NB, Canada.
RP Yang, YM (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
EM oscar.yang@jpl.nasa.gov
NR 23
TC 7
Z9 7
U1 2
U2 9
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 MAY
PY 2014
VL 49
IS 5
BP 341
EP 350
DI 10.1002/2013RS005344
PG 10
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA AJ4EN
UT WOS:000337624700004
ER
PT J
AU Manney, GL
Hegglin, MI
Daffer, WH
Schwartz, MJ
Santee, ML
Pawson, S
AF Manney, Gloria L.
Hegglin, Michaela I.
Daffer, William H.
Schwartz, Michael J.
Santee, Michelle L.
Pawson, Steven
TI Climatology of Upper Tropospheric-Lower Stratospheric (UTLS) Jets and
Tropopauses in MERRA
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Atmospheric circulation; Jets; Stratophere-troposphere coupling;
Tropopause; Upper troposphere; Data assimilation
ID EDDY-DRIVEN JET; NORTHERN-HEMISPHERE WINTER; BREAKING ROSSBY WAVES;
POLAR VORTEX; SOUTHERN-HEMISPHERE; TROPICAL PACIFIC; DECADAL CHANGES;
WESTERLY JET; WATER-VAPOR; OZONE LOSS
AB A global climatology (1979-2012) from the Modern-Era Retrospective Analysis for Research and Applications (MERRA) shows distributions and seasonal evolution of upper tropospheric jets and their relationships to the stratospheric subvortex and multiple tropopauses. The overall climatological patterns of upper tropospheric jets confirm those seen in previous studies, indicating accurate representation of jet stream dynamics in MERRA. The analysis shows a Northern Hemisphere (NH) upper tropospheric jet stretching nearly zonally from the mid-Atlantic across Africa and Asia. In winter-spring, this jet splits over the eastern Pacific, merges again over eastern North America, and then shifts poleward over the North Atlantic. The jets associated with tropical circulations are also captured, with upper tropospheric westerlies demarking cyclonic flow downstream from the Australian and Asian monsoon anticyclones and associated easterly jets. Multiple tropopauses associated with the thermal tropopause break commonly extend poleward from the subtropical upper tropospheric jet. In Southern Hemisphere (SH) summer, the tropopause break, along with a poleward-stretching secondary tropopause, often occurs across the tropical westerly jet downstream of the Australian monsoon region. SH high-latitude multiple tropopauses, nearly ubiquitous in June-July, are associated with the unique polar winter thermal structure. High-latitude multiple tropopauses in NH fall-winter are, however, sometimes associated with poleward-shifted upper tropospheric jets. The SH subvortex jet extends down near the level of the subtropical jet core in winter and spring. Most SH subvortex jets merge with an upper tropospheric jet between May and December; although much less persistent than in the SH, merged NH subvortex jets are common between November and April.
C1 [Manney, Gloria L.] NorthWest Res Associates, Socorro, NM USA.
[Manney, Gloria L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA.
[Hegglin, Michaela I.] Univ Reading, Reading, Berks, England.
[Daffer, William H.; Schwartz, Michael J.; Santee, Michelle L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Pawson, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Manney, GL (reprint author), New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
EM manney@nwra.com
RI Pawson, Steven/I-1865-2014; Hegglin, Michaela/D-7528-2017
OI Pawson, Steven/0000-0003-0200-717X; Hegglin,
Michaela/0000-0003-2820-9044
FU National Aeronautics and Space Administration
FX Thanks to the MLS team at JPL, especially Nathaniel Livesey, Brian
Knosp, Ryan Fuller, Vince Perun, and Robert Thurstans, for scientific,
data management/processing, and computational support. Thanks to NASA's
High-End Computing Program for computational resources used for MERRA,
to Michele Rienecker and other colleagues at NASA's GMAO for their
advice on using MERRA, and to the Goddard DAAC for distributing the
data. Thanks to Dennis Hartmann, Brian Hoskins, Kirstin Kruger, Ken
Minschwaner, Dave Raymond, Ted Shepherd, and Gui-Ying Yang for helpful
discussions. Thanks to the three anonymous reviewers for very helpful
comments. Work at the Jet Propulsion Laboratory, California Institute of
Technology, was done under contract with the National Aeronautics and
Space Administration.
NR 100
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Z9 8
U1 3
U2 19
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 MAY
PY 2014
VL 27
IS 9
BP 3248
EP 3271
DI 10.1175/JCLI-D-13-00243.1
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AI9RU
UT WOS:000337272700007
ER
PT J
AU Phojanamongkolkij, N
Kato, S
Wielicki, BA
Taylor, PC
Mlynczak, MG
AF Phojanamongkolkij, Nipa
Kato, Seiji
Wielicki, Bruce A.
Taylor, Patrick C.
Mlynczak, Martin G.
TI A Comparison of Climate Signal Trend Detection Uncertainty Analysis
Methods
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Climate records; Forecasting techniques; Statistical forecasting; Model
comparison
ID ENERGY SYSTEM INSTRUMENT; RADIATION BUDGET; CLOUDS; MODELS; OZONE
AB Two climate signal trend analysis methods are the focus of this paper. The uncertainty of trend estimate from these two methods is investigated using Monte Carlo simulation. Several theoretically and randomly generated series of white noise, first-order autoregressive and second-order autoregressive, are explored. The choice of method that is most appropriate for the time series of interest depends upon the autocorrelation structure of the series. If the structure has its autocorrelation coefficients decreased with increasing lags (i.e., an exponential decay pattern), then the method of Weatherhead et al. is adequate. If the structure exhibits a decreasing sinusoid pattern of coefficient with lags (or a damped sinusoid pattern) or a mixture of both exponential decay and damped sinusoid patterns, then the method of Leroy et al. is recommended. The two methods are then applied to the time series of monthly and globally averaged top-of-the-atmosphere (TOA) irradiances for the reflected solar shortwave and emitted longwave regions, using radiance observations made by Clouds and the Earth's Radiant Energy System (CERES) instruments during March 2000 through June 2011. Examination of the autocorrelation structures indicates that the reflected shortwave region has an exponential decay pattern, while the longwave region has a mixture of exponential decay and damped sinusoid patterns. Therefore, it is recommended that the method of Weatherhead et al. is used for the series of reflected shortwave irradiances and that the method of Leroy et al. is used for the series of emitted longwave irradiances.
C1 [Phojanamongkolkij, Nipa] NASA, Langley Res Ctr, Syst Engn & Engn Methods Branch, Hampton, VA 23681 USA.
[Kato, Seiji; Wielicki, Bruce A.; Taylor, Patrick C.; Mlynczak, Martin G.] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
RP Phojanamongkolkij, N (reprint author), NASA, Langley Res Ctr, MS 131, Hampton, VA 23681 USA.
EM nipa.phojanamongkolkij@nasa.gov
RI Taylor, Patrick/D-8696-2015; Richards, Amber/K-8203-2015
OI Taylor, Patrick/0000-0002-8098-8447;
FU NASA CLARREO project
FX We thank Dr. Stephen Leroy for useful discussions and all reviewers'
comments for valuable insights. We also thank Ms. Amber Richards and Dr.
Joe A. Walker for proof reading the manuscript. This work is supported
by the NASA CLARREO project.
NR 18
TC 0
Z9 0
U1 0
U2 9
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 MAY
PY 2014
VL 27
IS 9
BP 3363
EP 3376
DI 10.1175/JCLI-D-13-00400.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AI9RU
UT WOS:000337272700013
ER
PT J
AU Iizumi, T
Luo, JJ
Challinor, AJ
Sakurai, G
Yokozawa, M
Sakuma, H
Brown, ME
Yamagata, T
AF Iizumi, Toshichika
Luo, Jing-Jia
Challinor, Andrew J.
Sakurai, Gen
Yokozawa, Masayuki
Sakuma, Hirofumi
Brown, Molly E.
Yamagata, Toshio
TI Impacts of El Nino Southern Oscillation on the global yields of major
crops
SO NATURE COMMUNICATIONS
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; INDIAN-OCEAN; DIPOLE MODE; CLIMATE; PREDICTION;
PATTERNS; AGRICULTURE
AB The monitoring and prediction of climate-induced variations in crop yields, production and export prices in major food-producing regions have become important to enable national governments in import-dependent countries to ensure supplies of affordable food for consumers. Although the El Nino/Southern Oscillation (ENSO) often affects seasonal temperature and precipitation, and thus crop yields in many regions, the overall impacts of ENSO on global yields are uncertain. Here we present a global map of the impacts of ENSO on the yields of major crops and quantify its impacts on their global-mean yield anomalies. Results show that El Nino likely improves the global-mean soybean yield by 2.1-5.4% but appears to change the yields of maize, rice and wheat by - 4.3 to +0.8%. The global-mean yields of all four crops during La Nina years tend to be below normal (- 4.5 to 0.0%). Our findings highlight the importance of ENSO to global crop production.
C1 [Iizumi, Toshichika; Sakurai, Gen] Natl Inst Agroenvironm Sci, Tsukuba, Ibaraki 3058604, Japan.
[Luo, Jing-Jia] Bur Meteorol, Ctr Australian Weather & Climate Res, Melbourne, Vic 3008, Australia.
[Challinor, Andrew J.] Univ Leeds, Inst Climate & Atmospher Sci, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Challinor, Andrew J.] Univ Copenhagen, CGIAR ESSP Program Climate Change, Agr & Food Secur CCAFS, Dept Plant & Environm Sci,Fac Sci, DK-1958 Frederiksberg, Denmark.
[Yokozawa, Masayuki] Shizuoka Univ, Grad Sch Engn, Hamamatsu, Shizuoka 4328561, Japan.
[Sakuma, Hirofumi] JAMSTEC, Yokohama Inst Earth Sci, Res Inst Global Change, Yokohama, Kanagawa 2360001, Japan.
[Sakuma, Hirofumi; Yamagata, Toshio] JAMSTEC, Yokohama Inst Earth Sci, Applicat Lab, Yokohama, Kanagawa 2360001, Japan.
[Brown, Molly E.] NASA Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
RP Iizumi, T (reprint author), Natl Inst Agroenvironm Sci, Tsukuba, Ibaraki 3058604, Japan.
EM iizumit@affrc.go.jp
RI Brown, Molly/M-5146-2013; Yamagata, Toshio/A-1807-2009; Luo,
Jing-Jia/B-2481-2008; Yokozawa, Masayuki/O-2829-2014; Challinor,
Andrew/C-4992-2008; Brown, Molly/E-2724-2010
OI Brown, Molly/0000-0001-7384-3314; Luo, Jing-Jia/0000-0003-2181-0638;
Yokozawa, Masayuki/0000-0001-7053-2465; Challinor,
Andrew/0000-0002-8551-6617; Brown, Molly/0000-0001-7384-3314
FU Environment Research and Technology Development Fund of the Ministry of
the Environment, Japan [S-10-2]
FX We thank P. McIntosh and T. Beer for their comments. T.I and G.S. were
supported by the Environment Research and Technology Development Fund
(S-10-2) of the Ministry of the Environment, Japan.
NR 44
TC 22
Z9 22
U1 4
U2 61
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 MAY
PY 2014
VL 5
AR 3712
DI 10.1038/ncomms4712
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AJ0SB
UT WOS:000337365100001
PM 24827075
ER
PT J
AU Datta, DP
Sen, S
AF Datta, Dhurjati Prasad
Sen, Sudip
TI Excitation of flow instabilities due to nonlinear scale invariance
SO PHYSICS OF PLASMAS
LA English
DT Article
ID MULTIFRACTAL ANALYSIS; PLASMA; INTERMITTENCY; TURBULENCE; DYNAMICS; TIME
AB A novel route to instabilities and turbulence in fluid and plasma flows is presented in kinetic Vlasov-Maxwell model. New kind of flow instabilities is shown to arise due to the availability of new kinetic energy sources which are absent in conventional treatments. The present approach is based on a scale invariant nonlinear analytic formalism developed to address irregular motions on a chaotic attractor or in turbulence in a more coherent manner. We have studied two specific applications of this turbulence generating mechanism. The warm plasma Langmuir wave dispersion relation is shown to become unstable in the presence of these multifractal measures. In the second application, these multifractal measures are shown to induce naturally non-Gaussian, i.e., a stretched, Gaussian distribution and anomalous transport for tracer particles from the turbulent advection-diffusion transport equation in a Vlasov plasma flow. (C) 2014 AIP Publishing LLC.
C1 [Datta, Dhurjati Prasad] Univ N Bengal, Dept Math, Siliguri 734013, W Bengal, India.
[Sen, Sudip] NASA, Natl Inst Aerosp, LaRC, Hampton, VA 23666 USA.
[Sen, Sudip] Coll William & Mary, Williamsburg, VA 23187 USA.
RP Datta, DP (reprint author), Univ N Bengal, Dept Math, Siliguri 734013, W Bengal, India.
EM dp_datta@yahoo.com
NR 22
TC 1
Z9 1
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD MAY
PY 2014
VL 21
IS 5
AR 052311
DI 10.1063/1.4880103
PG 10
WC Physics, Fluids & Plasmas
SC Physics
GA AI7UY
UT WOS:000337107200027
ER
PT J
AU Jorns, BA
Hofer, RR
AF Jorns, Benjamin A.
Hofer, Richard R.
TI Plasma oscillations in a 6-kW magnetically shielded Hall thruster
SO PHYSICS OF PLASMAS
LA English
DT Article
ID HOLLOW-CATHODE; DISCHARGE; INSTABILITY; DRIFT
AB Plasma oscillations from 0-100 kHz in a 6-kW magnetically shielded Hall thruster are experimentally characterized with a high-speed, optical camera. Two modes are identified at 7-12 kHz and 70-90 kHz. The low frequency mode is found to be azimuthally uniform across the thruster face, while the high frequency oscillation is peaked close to the centerline-mounted cathode with an m 1 azimuthal dependence. An analysis of these results in the context of wave-based theory suggests that the low frequency wave is the breathing mode oscillation, while the higher frequency mode is gradient-driven. The effect of these oscillations on thruster operation is examined through an analysis of thruster discharge current and a comparison with published observations from an unshielded variant of the thruster. Most notably, it is found that although the oscillation spectra of the two thrusters are different, they exhibit nearly identical steady-state behavior. (C) 2014 AIP Publishing LLC.
C1 [Jorns, Benjamin A.; Hofer, Richard R.] CALTECH, Jet Prop Lab, Elect Prop Grp, Pasadena, CA 91109 USA.
RP Jorns, BA (reprint author), CALTECH, Jet Prop Lab, Elect Prop Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM benjamin.a.jorns@jpl.nasa.gov
FU In-Space Propulsion Technologies program
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 and
funded through the In-Space Propulsion Technologies program. The authors
would like to acknowledge Ray Swindlehurst and Nowell Niblitt for their
assistance in running the experimental facility. We are also grateful to
Dr. Dan Goebel and Dr. Ioannis Mikellides for providing data on the H6MS
and to Michael Sekerak for his assistance in understanding the FASTCAM
algorithms developed at the University of Michigan.
NR 54
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U1 0
U2 9
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD MAY
PY 2014
VL 21
IS 5
AR 053512
DI 10.1063/1.4879819
PG 11
WC Physics, Fluids & Plasmas
SC Physics
GA AI7UY
UT WOS:000337107200072
ER
PT J
AU Ni, XL
Park, T
Choi, SH
Shi, YL
Cao, CX
Wang, XJ
Lefsky, MA
Simard, M
Myneni, RB
AF Ni, Xiliang
Park, Taejin
Choi, Sungho
Shi, Yuli
Cao, Chunxiang
Wang, Xuejun
Lefsky, Michael A.
Simard, Marc
Myneni, Ranga B.
TI Allometric Scaling and Resource Limitations Model of Tree Heights: Part
3. Model Optimization and Testing over Continental China
SO REMOTE SENSING
LA English
DT Article
DE tree height; allometric scaling law; resource limitation; model
optimization; geoscience laser altimeter system (GLAS); national forest
inventory (NFI)
ID SPATIAL INTERPOLATION; VEGETATION STRUCTURE; SURFACE-TOPOGRAPHY;
TROPICAL FORESTS; DIAMETER MODELS; WATER RELATIONS; CANOPY HEIGHT;
WAVE-FORMS; CLIMATE; LIDAR
AB The ultimate goal of our multi-article series is to demonstrate the Allometric Scaling and Resource Limitation (ASRL) approach for mapping tree heights and biomass. This third article tests the feasibility of the optimized ASRL model over China at both site (14 meteorological stations) and continental scales. Tree heights from the Geoscience Laser Altimeter System (GLAS) waveform data are used for the model optimizations. Three selected ASRL parameters (area of single leaf, a; exponent for canopy radius, eta; and root absorption efficiency, gamma) are iteratively adjusted to minimize differences between the references and predicted tree heights. Key climatic variables (e.g., temperature, precipitation, and solar radiation) are needed for the model simulations. We also exploit the independent GLAS and in situ tree heights to examine the model performance. The predicted tree heights at the site scale are evaluated against the GLAS tree heights using a two-fold cross validation (RMSE = 1.72 m; R-2 = 0.97) and bootstrapping (RMSE = 4.39 m; R-2 = 0.81). The modeled tree heights at the continental scale (1 km spatial resolution) are compared to both GLAS (RMSE = 6.63 m; R-2 = 0.63) and in situ (RMSE = 6.70 m; R-2 = 0.52) measurements. Further, inter-comparisons against the existing satellite-based forest height maps have resulted in a moderate degree of agreements. Our results show that the optimized ASRL model is capable of satisfactorily retrieving tree heights over continental China at both scales. Subsequent studies will focus on the estimation of woody biomass after alleviating the discussed limitations.
C1 [Ni, Xiliang; Cao, Chunxiang] Chinese Acad Sci, Inst Remote Sensing & Digital Earth, State Key Lab Remote Sensing Sci, Beijing 100101, Peoples R China.
[Ni, Xiliang; Park, Taejin; Choi, Sungho; Shi, Yuli; Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Shi, Yuli] Nanjing Univ Informat Sci & Technol, Sch Remote Sensing, Nanjing 210044, Jiangsu, Peoples R China.
[Wang, Xuejun] State Forest Adm China, Survey Planning & Design Inst, Beijing 100714, Peoples R China.
[Lefsky, Michael A.] Colorado State Univ, Nat Resource Ecol Lab, Ctr Ecol Anal Lidar, Ft Collins, CO 80523 USA.
[Simard, Marc] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Park, T (reprint author), Boston Univ, Dept Earth & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA.
EM nixl@irsa.ac.cn; partj@bu.edu; schoi@bu.edu; ylshi.nuist@gmail.com;
cao413@irsa.ac.cn; wangxuejun320@126.com; lefsky@cnr.colostate.edu;
marc.simard@jpl.nasa.gov; ranga.myneni@gmail.com
RI Myneni, Ranga/F-5129-2012; Simard, Marc/H-3516-2013
OI Simard, Marc/0000-0002-9442-4562
FU National high Technology Research and Development Program of China (863
Program) [2013AA12A302]; Fulbright Program for graduate studies; NASA
Headquarters under the NASA Earth and Space Science Fellowship
Program-Grant [NNX13AP55H]
FX The authors would like to thank Joshua Mantooth for his helpful review
of this paper. Thanks also to the three anonymous reviewers whose
comments significantly improved this manuscript. This study was
partially funded by the National high Technology Research and
Development Program of China (863 Program) (Grand No. 2013AA12A302).
This work was also supported by the Fulbright Program for graduate
studies and NASA Headquarters under the NASA Earth and Space Science
Fellowship Program-Grant "NNX13AP55H".
NR 56
TC 4
Z9 4
U1 2
U2 21
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD MAY
PY 2014
VL 6
IS 5
BP 3533
EP 3553
DI 10.3390/rs6053533
PG 21
WC Remote Sensing
SC Remote Sensing
GA AI8JW
UT WOS:000337160700001
ER
PT J
AU Wentz, EA
Anderson, S
Fragkias, M
Netzband, M
Mesev, V
Myint, SW
Quattrochi, D
Rahman, A
Seto, KC
AF Wentz, Elizabeth A.
Anderson, Sharolyn
Fragkias, Michail
Netzband, Maik
Mesev, Victor
Myint, Soe W.
Quattrochi, Dale
Rahman, Atiqur
Seto, Karen C.
TI Supporting Global Environmental Change Research: A Review of Trends and
Knowledge Gaps in Urban Remote Sensing
SO REMOTE SENSING
LA English
DT Review
DE urban mapping; environmental indices; social indices; climate modeling;
socioeconomic modeling
ID LAND-SURFACE TEMPERATURE; NIGHTTIME SATELLITE IMAGERY; HIGH-RESOLUTION
SATELLITE; SPECTRAL MIXTURE ANALYSIS; BUILT-UP INDEX; IMPERVIOUS
SURFACE; HEAT-ISLAND; UNITED-STATES; COVER CLASSIFICATION;
POPULATION-DENSITY
AB This paper reviews how remotely sensed data have been used to understand the impact of urbanization on global environmental change. We describe how these studies can support the policy and science communities' increasing need for detailed and up-to-date information on the multiple dimensions of cities, including their social, biological, physical, and infrastructural characteristics. Because the interactions between urban and surrounding areas are complex, a synoptic and spatial view offered from remote sensing is integral to measuring, modeling, and understanding these relationships. Here we focus on three themes in urban remote sensing science: mapping, indices, and modeling. For mapping we describe the data sources, methods, and limitations of mapping urban boundaries, land use and land cover, population, temperature, and air quality. Second, we described how spectral information is manipulated to create comparative biophysical, social, and spatial indices of the urban environment. Finally, we focus how the mapped information and indices are used as inputs or parameters in models that measure changes in climate, hydrology, land use, and economics.
C1 [Wentz, Elizabeth A.; Myint, Soe W.] Arizona State Univ, Sch Geog Sci & Urban Planning, Tempe, AZ 85287 USA.
[Anderson, Sharolyn] Univ S Australia, Sch Nat & Built Environm, Adelaide, SA 5001, Australia.
[Fragkias, Michail] Boise State Univ, COBE, Dept Econ, Boise, ID 83725 USA.
[Netzband, Maik] Ruhr Univ Bochum, Dept Geog, D-44801 Bochum, Germany.
[Mesev, Victor] Florida State Univ, Dept Geog, Tallahassee, FL 32306 USA.
[Quattrochi, Dale] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA.
[Rahman, Atiqur] Jamia Millia Islamia, Dept Geog, New Delhi 110025, India.
[Seto, Karen C.] Yale Univ, Yale Sch Forestry & Environm Studies, New Haven, CT 06511 USA.
RP Wentz, EA (reprint author), Arizona State Univ, Sch Geog Sci & Urban Planning, Coor Hall,5th Floor,975 S Myrtle Ave, Tempe, AZ 85287 USA.
EM wentz@asu.edu; Sharolyn.Anderson@unisa.edu.au;
michailfragkias@boisestate.edu; maik.netzband@rub.de; vmesev@fsu.edu;
dale.quattrochi@nasa.gov; ateeqgeog@yahoo.co.in; karen.seto@yale.edu
RI Seto, Karen/C-2722-2008; Anderson, Sharolyn/F-4653-2013
OI Anderson, Sharolyn/0000-0002-9456-0193
FU NASA [NNX10AN11G]; National Science Foundation [GSS-023907]
FX This material is based upon work supported by NASA Grant No. NNX10AN11G
and the National Science Foundation Grant No. GSS-023907. Any opinions,
findings and conclusions, or recommendation expressed here are those of
the authors and do not necessarily reflect the views of the funding
agencies. The authors also acknowledge contributions from the
Forecasting Urban Land-use Change Workshop (NASA) and the Urban Remote
Sensing Workshop (NSF) participants: Rimjhim Aggarwal, Shlomo (Solly)
Angel, Philip Christensen, Keith Clarke, Richard Dawson, Fabio
Dell'Aqua, Xiangzheng Deng, Peter Omu Elias, Jonathan Fink, Tyler
Frazier, Arjit Guha, Subhro Guhathakurta, Burak Guneralp, Geoffrey
Henebry, Clair Jantz, Shai Kaplan, Donghwan Kim, Jose Lobo, Miguel
Luengo-Oroz, Jacqueline Lu, Darle Monroe, David Nelson, Robert (Gil)
Pontius, Milap Punia, Lela Preshad, Ray Quay, Charles Redman, Qing Shen,
Christopher Small, William Solecki, Tod Swanson, Scott Weisman, and
Sainan Zhang. We also acknowledge Cary Simmons and Qian Zhang for help
with graphics.
NR 162
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U1 9
U2 116
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD MAY
PY 2014
VL 6
IS 5
BP 3879
EP 3905
DI 10.3390/rs6053879
PG 27
WC Remote Sensing
SC Remote Sensing
GA AI8JW
UT WOS:000337160700017
ER
PT J
AU Lee, BC
Huang, W
Tao, L
Yamamoto, N
Gallimore, AD
Yalin, AP
AF Lee, B. C.
Huang, W.
Tao, L.
Yamamoto, N.
Gallimore, A. D.
Yalin, A. P.
TI A cavity ring-down spectroscopy sensor for real-time Hall thruster
erosion measurements
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
AB A continuous-wave cavity ring-down spectroscopy sensor for real-time measurements of sputtered boron from Hall thrusters has been developed. The sensor uses a continuous-wave frequency-quadrupled diode laser at 250 nm to probe ground state atomic boron sputtered from the boron nitride insulating channel. Validation results from a controlled setup using an ion beam and target showed good agreement with a simple finite-element model. Application of the sensor for measurements of two Hall thrusters, the H6 and SPT-70, is described. The H6 was tested at power levels ranging from 1.5 to 10 kW. Peak boron densities of 10 +/- 2 x 10(14) m (3) were measured in the thruster plume, and the estimated eroded channel volume agreed within a factor of 2 of profilometry. The SPT-70 was tested at 600 and 660 W, yielding peak boron densities of 7.2 +/- 1.1 x 10(14) m (3), and the estimated erosion rate agreed within similar to 20% of profilometry. Technical challenges associated with operating a high-finesse cavity in the presence of energetic plasma are also discussed. (C) 2014 AIP Publishing LLC.
C1 [Lee, B. C.] Colorado State Univ, Dept Phys, Ft Collins, CO 80521 USA.
[Huang, W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Tao, L.; Yamamoto, N.; Yalin, A. P.] Colorado State Univ, Dept Mech Engn, Ft Collins, CO 80521 USA.
[Gallimore, A. D.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA.
RP Yalin, AP (reprint author), Colorado State Univ, Dept Mech Engn, Ft Collins, CO 80521 USA.
EM ayalin@engr.colostate.edu
RI Tao, Lei/F-6793-2012
FU National Aeronautics and Space Administration (NASA) Space Technology
Research Fellowship [NX11AN30H]
FX The authors would like to acknowledge support from the National
Aeronautics and Space Administration (NASA) Space Technology Research
Fellowship Grant No. NX11AN30H.
NR 41
TC 3
Z9 3
U1 2
U2 17
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0034-6748
EI 1089-7623
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD MAY
PY 2014
VL 85
IS 5
AR 053111
DI 10.1063/1.4879135
PG 11
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA AI7UD
UT WOS:000337104600011
PM 24880357
ER
PT J
AU Tobiska, WK
Gersey, B
Wilkins, R
Mertens, C
Atwell, W
Bailey, J
AF Tobiska, W. Kent
Gersey, Brad
Wilkins, Richard
Mertens, Chris
Atwell, William
Bailey, Justin
TI Reply to comment by Rainer Facius et al. on "US Government shutdown
degrades aviation radiation monitoring during solar radiation storm"
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID INITIAL VALIDATION; MODEL DEVELOPMENT; DOSE CLIMATOLOGY
AB The premise of this comment perpetuates an unfortunate trend among some radiation researchers to minimize potential risks to human tissue from low-radiation sources. In fact, this discussion on the risk uncertainties of low-dose radiation further illustrates the need for more measurements and a program of active monitoring, especially when solar eruptive events can substantially elevate the radiation environment. This debate also highlights the context of a bigger problem; i.e., how do we as professionals act with due diligence to take the immense body of knowledge of space weather radiation effects on human tissue and distil it into ideas that regulatory agencies can use to maximize the safety of a population at risk. The focus of our article on radiation risks due to solar energetic particle events starts with our best assessment of risks and is based on the body of scientific knowledge while, at the same time, erring on the side of public safety. The uncertainty inherent in our assessment is accepted and described with this same philosophy in mind.
C1 [Tobiska, W. Kent; Bailey, Justin] Space Environm Technol, Pacific Palisades, CA 90272 USA.
[Gersey, Brad; Wilkins, Richard] Prairie View A&M Univ, Prairie View, TX USA.
[Mertens, Chris] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Atwell, William] Boeing Co, Houston, TX USA.
RP Tobiska, WK (reprint author), Space Environm Technol, Pacific Palisades, CA 90272 USA.
EM ktobiska@spacenvironment.net
NR 11
TC 1
Z9 1
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD MAY
PY 2014
VL 12
IS 5
BP 320
EP 321
DI 10.1002/2014SW001074
PG 2
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA AJ3BW
UT WOS:000337541100005
ER
PT J
AU Ade, PAR
Aghanim, N
Alves, MIR
Arnaud, M
Atrio-Barandela, F
Aumont, J
Baccigalupi, C
Banday, AJ
Barreiro, RB
Battaner, E
Benabed, K
Benoit-Levy, A
Bernard, JP
Bersanelli, M
Bielewicz, P
Bobin, J
Bonaldi, A
Bond, IR
Borrill, J
Bouchet, FR
Boulanger, E
Burigana, C
Cardoso, JF
Casassus, S
Catalano, A
Chamballu, A
Chen, X
Chiang, HC
Chiang, LY
Christensen, PR
Clements, DL
Colombi, S
Colombo, LPL
Couchot, F
Crill, BP
Cuttaia, F
Danese, L
Davies, RD
Davis, RJ
de Bernardis, P
de Rosa, A
de Zotti, G
Delabrouille, J
Desert, FX
Dickinson, C
Diego, JM
Donzelli, S
Dore, O
Dupac, X
Ensslin, TA
Eriksen, HK
Finelli, F
Forni, O
Franceschi, E
Galeotta, S
Ganga, K
Genova-Santos, RT
Ghosh, T
Giard, M
Gonzalez-Nuevo, J
Gorski, KM
Gregorio, A
Gruppuso, A
Hansen, EK
Harrison, DL
Helou, G
Hernandez-Monteagudo, C
Hildebrandt, SR
Hivon, E
Hobson, M
Hornstrup, A
Jaffe, AH
Jaffe, TR
Jones, WC
Keihanen, E
Keskitalo, R
Kneissl, R
Knoche, I
Kunz, M
Kurki-Suonio, H
Lahteenmaki, A
Lamarre, JM
Lasenby, A
Lawrence, CR
Leonardi, R
Liguori, M
Lilje, PB
Linden-Vornle, M
Lopez-Caniego, M
Macias-Perez, JF
Maffei, B
Maino, D
Mandolesi, N
Marshall, DJ
Martin, PG
Martinez-Gonzalez, E
Masi, S
Massardi, M
Matarrese, S
Mazzotta, P
Meinhold, PR
Melchiorri, A
Mendes, L
Mennella, A
Migliaccio, M
Miville-Deschenes, MA
Moneti, A
Montier, L
Morgante, G
Mortlock, D
Munshi, D
Naselsky, P
Nati, F
Natoli, P
Norgaard-Nielsen, HU
Noviello, F
Novikov, D
Novikov, I
Oxborrow, CA
Pagano, L
Pajot, F
Paladini, R
Paoletti, D
Patanchon, G
Pearson, TJ
Peel, M
Perdereau, O
Perrotta, F
Piacentini, F
Piat, M
Pierpaoli, E
Pietrobon, D
Plaszczynski, S
Pointecouteau, E
Polenta, G
Ponthieu, N
Popa, L
Pratt, GW
Prunet, S
Puget, JL
Rachen, JP
Rebolo, R
Reich, W
Reinecke, M
Remazeilles, M
Renault, C
Ricciardi, S
Riller, T
Ristorcelli, I
Rocha, G
Rosset, C
Roudier, G
Rubino-Martin, JA
Rusholme, B
Sandri, M
Savini, G
Scott, D
Spencer, D
Stolyarov, V
Sutton, D
Suur-Uski, AS
Sygnet, JF
Tauber, JA
Tavagnacco, D
Terenzi, L
Tibbs, CT
Toffolatti, L
Tomasi, M
Tristram, M
Tucci, M
Valenziano, L
Valiviita, J
Van Tent, B
Varis, J
Verstraete, L
Vielva, P
Villa, F
Wandelt, BD
Watson, R
Wilkinson, A
Ysard, N
Yvon, D
Zacchei, A
Zonca, A
AF Ade, P. A. R.
Aghanim, N.
Alves, M. I. R.
Arnaud, M.
Atrio-Barandela, F.
Aumont, J.
Baccigalupi, C.
Banday, A. J.
Barreiro, R. B.
Battaner, E.
Benabed, K.
Benoit-Levy, A.
Bernard, J-P
Bersanelli, M.
Bielewicz, P.
Bobin, J.
Bonaldi, A.
Bond, I. R.
Borrill, J.
Bouchet, F. R.
Boulanger, E.
Burigana, C.
Cardoso, J-F
Casassus, S.
Catalano, A.
Chamballu, A.
Chen, X.
Chiang, H. C.
Chiang, L-Y
Christensen, P. R.
Clements, D. L.
Colombi, S.
Colombo, L. P. L.
Couchot, F.
Crill, B. P.
Cuttaia, F.
Danese, L.
Davies, R. D.
Davis, R. J.
de Bernardis, P.
de Rosa, A.
de Zotti, G.
Delabrouille, J.
Desert, F-X
Dickinson, C.
Diego, J. M.
Donzelli, S.
Dore, O.
Dupac, X.
Ensslin, T. A.
Eriksen, H. K.
Finelli, F.
Forni, O.
Franceschi, E.
Galeotta, S.
Ganga, K.
Genova-Santos, R. T.
Ghosh, T.
Giard, M.
Gonzalez-Nuevo, J.
Gorski, K. M.
Gregorio, A.
Gruppuso, A.
Hansen, E. K.
Harrison, D. L.
Helou, G.
Hernandez-Monteagudo, C.
Hildebrandt, S. R.
Hivon, E.
Hobson, M.
Hornstrup, A.
Jaffe, A. H.
Jaffe, T. R.
Jones, W. C.
Keihanen, E.
Keskitalo, R.
Kneissl, R.
Knoche, I.
Kunz, M.
Kurki-Suonio, H.
Lahteenmaki, A.
Lamarre, J-M
Lasenby, A.
Lawrence, C. R.
Leonardi, R.
Liguori, M.
Lilje, P. B.
Linden-Vornle, M.
Lopez-Caniego, M.
Macias-Perez, J. F.
Maffei, B.
Maino, D.
Mandolesi, N.
Marshall, D. J.
Martin, P. G.
Martinez-Gonzalez, E.
Masi, S.
Massardi, M.
Matarrese, S.
Mazzotta, P.
Meinhold, P. R.
Melchiorri, A.
Mendes, L.
Mennella, A.
Migliaccio, M.
Miville-Deschenes, M-A
Moneti, A.
Montier, L.
Morgante, G.
Mortlock, D.
Munshi, D.
Naselsky, P.
Nati, F.
Natoli, P.
Norgaard-Nielsen, H. U.
Noviello, F.
Novikov, D.
Novikov, I.
Oxborrow, C. A.
Pagano, L.
Pajot, F.
Paladini, R.
Paoletti, D.
Patanchon, G.
Pearson, T. J.
Peel, M.
Perdereau, O.
Perrotta, F.
Piacentini, F.
Piat, M.
Pierpaoli, E.
Pietrobon, D.
Plaszczynski, S.
Pointecouteau, E.
Polenta, G.
Ponthieu, N.
Popa, L.
Pratt, G. W.
Prunet, S.
Puget, J-L
Rachen, J. P.
Rebolo, R.
Reich, W.
Reinecke, M.
Remazeilles, M.
Renault, C.
Ricciardi, S.
Riller, T.
Ristorcelli, I.
Rocha, G.
Rosset, C.
Roudier, G.
Rubino-Martin, J. A.
Rusholme, B.
Sandri, M.
Savini, G.
Scott, D.
Spencer, D.
Stolyarov, V.
Sutton, D.
Suur-Uski, A-S
Sygnet, J-F
Tauber, J. A.
Tavagnacco, D.
Terenzi, L.
Tibbs, C. T.
Toffolatti, L.
Tomasi, M.
Tristram, M.
Tucci, M.
Valenziano, L.
Valiviita, J.
Van Tent, B.
Varis, J.
Verstraete, L.
Vielva, P.
Villa, F.
Wandelt, B. D.
Watson, R.
Wilkinson, A.
Ysard, N.
Yvon, D.
Zacchei, A.
Zonca, A.
CA Planck Collaboration
TI Planck intermediate results. XV. A study of anomalous microwave emission
in Galactic clouds
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE HII regions; radiation mechanisms: general; radio continuum: ISM;
submillimeter: ISM
ID SPINNING DUST EMISSION; PROBE WMAP OBSERVATIONS; H-II REGIONS;
PRE-LAUNCH STATUS; CENTIMETER-WAVE CONTINUUM; GHZ SKY SURVEY;
ANISOTROPY-PROBE; MOLECULAR CLOUDS; FOREGROUND EMISSION; STAR-FORMATION
AB Anomalous microwave emission (AME) is believed to be due to electric dipole radiation from small spinning dust grains. The aim of this paper is a statistical study of the basic properties of AME regions and the environment in which they emit. We used WMAP and Planck maps, combined with ancillary radio and IR data, to construct a sample of 98 candidate AME sources, assembling SEDs for each source using aperture photometry on 1 degrees-smoothed maps from 0.408 GHz up to 3000 GHz. Each spectrum is fitted with a simple model of free-free, synchrotron (where necessary), cosmic microwave background (CMB), thermal dust, and spinning dust components. We find that 42 of the 98 sources have significant (>5 sigma) excess emission at frequencies between 20 and 60 GHz. An analysis of the potential contribution of optically thick free-free emission from ultra-compact H II regions, using IR colour criteria, reduces the significant AME sample to 27 regions. The spectrum of the AME is consistent with model spectra of spinning dust. Peak frequencies are in the range 20-35 GHz except for the California nebula (NGC1499), which appears to have a high spinning dust peak frequency of (50 +/- 17) GHz. The AME regions tend to be more spatially extended than regions with little or no AME. The AME intensity is strongly correlated with the sub-millimetre/IR flux densities and comparable to previous AME detections in the literature. AME emissivity, defined as the ratio of AME to dust optical depth, varies by an order of magnitude for the AME regions. The AME regions tend to be associated with cooler dust in the range 14-20K and an average emissivity index, beta(d), of + 1.8, while the non-AME regions are typically warmer, at 20-27 K. In agreement with previous studies, the AME emissivity appears to decrease with increasing column density. This supports the idea of AME originating from small grains that are known to be depleted in dense regions, probably due to coagulation onto larger grains. We also find a correlation between the AME emissivity (and to a lesser degree the spinning dust peak frequency) and the intensity of the interstellar radiation field, G(0). Modelling of this trend suggests that both radiative and collisional excitation are important for the spinning dust emission. The most significant AME regions tend to have relatively less ionized gas (free-free emission), although this could be a selection effect. The infrared excess, a measure of the heating of dust associated with H II regions, is typically >4 for AME sources, indicating that the dust is not primarily heated by hot OB stars. The AME regions are associated with known dark nebulae and have higher 12 mu m/25 mu m ratios. The emerging picture is that the bulk of the AME is coming from the polycyclic aromatic hydrocarbons and small dust grains from the colder neutral interstellar medium phase.
C1 [Cardoso, J-F; Delabrouille, J.; Ganga, K.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.] Univ Paris Diderot, APC, Sorbonne Paris Cite, CNRS,IN2P3,CEA,Irfu,Observ Paris, F-75205 Paris 13, France.
[Lahteenmaki, A.] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland.
[Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, Aalto 00076, Finland.
[Kunz, M.] African Inst Math Sci, ZA-7950 Cape Town, South Africa.
[Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy.
[Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy.
[Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Astrophys Grp, Cavendish Lab, Cambridge CB3 0HE, England.
[Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa.
[Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile.
[Bond, I. R.; Martin, P. G.; Miville-Deschenes, M-A] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Banday, A. J.; Bernard, J-P; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Crill, B. P.; Dore, O.; Helou, G.; Hildebrandt, S. R.; Pearson, T. J.; 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, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Rebolo, R.] CSIC, Madrid, Spain.
[Chamballu, A.; 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, Denmark.
[Kunz, M.; Tucci, 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, Dept Astrophys, IMAPP, 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, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA.
[Benoit-Levy, A.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Keihanen, E.; Kurki-Suonio, H.; Suur-Uski, A-S; Valiviita, J.; Ysard, N.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Chiang, H. C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA.
[Liguori, M.; 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.; Pagano, L.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Bersanelli, M.; Maino, D.; Mennella, A.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy.
[Gregorio, A.; Tavagnacco, D.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, 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, E-38206 Tenerife, Spain.
[Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile.
[Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid 28692, Spain.
[Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands.
[Kurki-Suonio, H.; Lahteenmaki, A.; Suur-Uski, A-S; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland.
[de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Galeotta, S.; Gregorio, A.; Tavagnacco, D.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Massardi, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Burigana, C.; Cuttaia, F.; de Rosa, A.; 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, I-40129 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.; Pagano, L.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy.
[Gregorio, A.] INFN Natl Inst Nucl Phys, I-34127 Trieste, Italy.
[Desert, F-X; Ponthieu, N.] Univ Grenoble 1, IPAG, Grenoble CNRS INSU 1, UMR 5274, F-38041 Grenoble, France.
[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.
[Chen, X.; Paladini, R.; Pearson, T. J.; Rusholme, B.; Tibbs, C. T.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Aghanim, N.; Alves, M. I. R.; Aumont, J.; Boulanger, E.; Chamballu, A.; Ghosh, T.; Kunz, M.; Miville-Deschenes, M-A; Pajot, F.; Ponthieu, N.; Puget, J-L; Remazeilles, M.; Verstraete, L.] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR8617, F-91405 Orsay, France.
[Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J-F; Colombi, S.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J-F; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France.
[Popa, L.] Inst Space Sci, Bucharest, Romania.
[Chiang, L-Y] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Harrison, D. L.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Eriksen, H. K.; Hansen, E. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, N-0313 Oslo, Norway.
[Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Barreiro, R. B.; Diego, J. M.; Gonzalez-Nuevo, J.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain.
[Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Lawrence, C. R.; Pietrobon, D.; Rocha, G.; Roudier, G.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bonaldi, A.; Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.; Noviello, F.; Peel, M.; Remazeilles, M.; Watson, R.; Wilkinson, A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Harrison, D. L.; Lasenby, A.; Migliaccio, M.; Stolyarov, V.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
[Couchot, F.; Perdereau, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, CNRS, IN2P3, LAL, F-91405 Orsay, France.
[Catalano, A.; Lamarre, J-M; Roudier, G.] Observ Paris, CNRS, LERMA, F-75014 Paris, France.
[Arnaud, M.; Bobin, J.; Chamballu, A.; Marshall, D. J.; Pratt, G. W.] Univ Paris Diderot, CEA Saclay, Lab AIM, IRFU,Serv Astrophys,CEA,DSM,CNRS, F-91191 Gif Sur Yvette, France.
[Cardoso, J-F] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris, France.
[Cardoso, J-F] Telecom ParisTech, F-75634 Paris, France.
[Catalano, A.; Macias-Perez, J. F.; Renault, C.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, Inst Natl Polytech Grenoble, CNRS,IN2P3, 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.
[Ensslin, T. A.; Hernandez-Monteagudo, C.; Knoche, I.; Rachen, J. P.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Reich, W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo 02044, Finland.
[Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Savini, G.] UCL, Opt Sci Lab, London WC1E 6BT, England.
[Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Ade, P. A. R.; Munshi, D.; Spencer, D.] 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, Arkhyz 369167, Zelenchukskiy R, Russia.
[Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR 7095, F-75014 Paris, France.
[Casassus, S.] Univ Santiago Chile, Santiago, Chile.
[Banday, A. J.; Bernard, J-P; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Dickinson, C (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England.
EM clive.dickinson@manchester.ac.uk
RI Remazeilles, Mathieu/N-1793-2015; Bobin, Jerome/P-3729-2014; Stolyarov,
Vladislav/C-5656-2017; Valiviita, Jussi/A-9058-2016; Mazzotta,
Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Ghosh,
Tuhin/E-6899-2016; Tomasi, Maurizio/I-1234-2016; Casassus,
Simon/I-8609-2016; 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; Lahteenmaki, Anne/L-5987-2013; Toffolatti,
Luigi/K-5070-2014; Lopez-Caniego, Marcos/M-4695-2013; Battaner,
Eduardo/P-7019-2014; Vielva, Patricio/F-6745-2014; Gruppuso,
Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Barreiro, Rita
Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez,
Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Pearson,
Timothy/N-2376-2015;
OI de Bernardis, Paolo/0000-0001-6547-6446; Remazeilles,
Mathieu/0000-0001-9126-6266; Matarrese, Sabino/0000-0002-2573-1243;
Galeotta, Samuele/0000-0002-3748-5115; WANDELT,
Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Scott,
Douglas/0000-0002-6878-9840; Lopez-Caniego, Marcos/0000-0003-1016-9283;
Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147;
Savini, Giorgio/0000-0003-4449-9416; Pierpaoli,
Elena/0000-0002-7957-8993; Villa, Fabrizio/0000-0003-1798-861X; TERENZI,
LUCA/0000-0001-9915-6379; Watson, Robert/0000-0002-5873-0124; Zacchei,
Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Bobin,
Jerome/0000-0003-1457-7890; Stolyarov, Vladislav/0000-0001-8151-828X;
Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti,
Gianfranco/0000-0003-2868-2595; Sandri, Maura/0000-0003-4806-5375;
Franceschi, Enrico/0000-0002-0585-6591; Valenziano,
Luca/0000-0002-1170-0104; Morgante, Gianluca/0000-0001-9234-7412; Peel,
Mike/0000-0003-3412-2586; Masi, Silvia/0000-0001-5105-1439; Valiviita,
Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748;
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; Toffolatti,
Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X;
Gruppuso, Alessandro/0000-0001-9272-5292; Barreiro, Rita
Belen/0000-0002-6139-4272; Martinez-Gonzalez,
Enrique/0000-0002-0179-8590; Gonzalez-Nuevo,
Joaquin/0000-0003-1354-6822; Pearson, Timothy/0000-0001-5213-6231;
Gregorio, Anna/0000-0003-4028-8785; Polenta,
Gianluca/0000-0003-4067-9196; Cuttaia, Francesco/0000-0001-6608-5017;
Burigana, Carlo/0000-0002-3005-5796; Bouchet,
Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043
FU NASA Office of Space Science; National Aeronautics and Space
Administration; STFC Advanced Fellowship; EU; ERC [307209]; ESA; CNES
(France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF
(Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain);
MICINN (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland);
CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space
(Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES
(Portugal); PRACE (EU)
FX We thank the anonymous referee for providing useful comments. We thank
Justin Jonas for providing the 2326 MHz HartRAO map. We acknowledge the
use of the MPIfR Survey Sampler website at
http://www.mpifr-bonn.mpg.de/survey.html and the Legacy Archive for
Microwave Background Data Analysis (LAMBDA); support for LAMBDA is
provided by the NASA Office of Space Science. 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 also makes use of the SIMBAD database, operated at the CDS,
Strasbourg, France. We acknowledge the use of NASA's SkyView facility
(http://skyview.gsfc.nasa.gov) located at NASA Goddard Space Flight
Center. C. D. acknowledges an STFC Advanced Fellowship, an EU
Marie-Curie IRG grant under the FP7, and an ERC Starting Grant (No.
307209). 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&page=Planck_Collabora
tion
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FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2014
VL 565
AR A103
DI 10.1051/0004-6361/201322612
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI3AN
UT WOS:000336730900103
ER
PT J
AU Bitsakis, T
Charmandaris, V
Appleton, PN
Diaz-Santos, T
Le Floc'h, E
da Cunha, E
Alatalo, K
Cluver, M
AF Bitsakis, T.
Charmandaris, V.
Appleton, P. N.
Diaz-Santos, T.
Le Floc'h, E.
da Cunha, E.
Alatalo, K.
Cluver, M.
TI Herschel observations of Hickson compact groups of galaxies: Unveiling
the properties of cold dust
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: evolution; galaxies: interactions; galaxies: groups: general;
infrared: galaxies
ID STEPHANS QUINTET; STAR-FORMATION; NEARBY GALAXIES; MOLECULAR GAS;
SUBMILLIMETER PHOTOMETRY; INFRARED PROPERTIES; NEUTRAL HYDROGEN; NUCLEAR
ACTIVITY; VIRGO CLUSTER; GREEN VALLEY
AB We present a Herschel far-infrared and sub-millimetre (sub-mm) study of a sample of 120 galaxies in 28 tlickson compact groups (HCGs). Fitting their UV to sub-mm spectral energy distributions with the model of da Cunha et al. (2008), we accurately estimate the dust masses, luminosities, and temperatures of the individual galaxies. We find that nearly half of the late-type galaxies in dynamically "old" groups, those with more than 25% of early-type members and redder UV-optical colours, also have significantly lower dust-to-stellar mass ratios compared to those of actively star-forming galaxies of the same mass found both in HCGs and in the field. Examining their dust-to-gas mass ratios, we conclude that dust was stripped out of these systems as a result of the gravitational and hydrodynamic interactions, experienced owing to previous encounters with other group members. About 40% of the early-type galaxies (mostly lenticulars), in dynamically "old" groups, display dust properties similar to those of the UV-optical red late-type galaxies. Given their stellar masses, star formation rates, and UV-optical colours, we suggest that red late-type and dusty lenticular galaxies represent transition populations between blue star-forming disk galaxies and quiescent early-type ellipticals. On the other hand, both the complete absence of any correlation between the dust and stellar masses of the dusty ellipticals and their enhanced star formation activity, suggest the increase in their gas and dust content due to accretion and merging. Our deep Herschel observations also allow us to detect the presence of diffuse cold intragroup dust in 4 HCGs. We also find that the fraction of 250 mu m emission that is located outside of the main bodies of both the red late-type galaxies and the dusty lenticulars is 15-20% of their integrated emission at this band. All these findings are consistent with an evolutionary scenario in which gas dissipation, shocks, and turbulence, in addition to tidal interactions, shape the evolution of galaxies in compact groups.
C1 [Bitsakis, T.; Charmandaris, V.] Univ Crete, Dept Phys, Iraklion 71003, Greece.
[Bitsakis, T.; Appleton, P. N.; Alatalo, K.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Bitsakis, T.] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Greece.
[Charmandaris, V.] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, Penteli 15236, Greece.
[Charmandaris, V.] Observ Paris, F-75014 Paris, France.
[Diaz-Santos, T.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Le Floc'h, E.] CEA Saclay, F-91191 Gif Sur Yvette, France.
[da Cunha, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Cluver, M.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa.
RP Bitsakis, T (reprint author), Univ Crete, Dept Phys, Iraklion 71003, Greece.
EM bitsakis@physics.uoc.gr
RI Charmandaris, Vassilis/A-7196-2008; Bitsakis, Theodoros/O-2766-2013;
OI Charmandaris, Vassilis/0000-0002-2688-1956; Bitsakis,
Theodoros/0000-0001-5787-8242; Appleton, Philip/0000-0002-7607-8766; da
Cunha, Elisabete/0000-0001-9759-4797
FU EU [PIRSES-GA-2012-316788]; NASA
FX T.B. and V.C. would like to acknowledge partial support from the EU FP7
Grant PIRSES-GA-2012-316788. This work is based, in part, on
observations made with Herschel, a European Space Agency Cornerstone
Mission with significant participation by NASA. Support for this work
was also provided by NASA through an award issued by JPL/Caltech. We
also appreciate the very useful comments of the referee, A. Boseili,
which helped improve this paper. Finally, we are grateful to L.
Verdes-Montenegro for providing the HI moment-0 maps of 4 HCGs.
NR 82
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FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2014
VL 565
AR A25
DI 10.1051/0004-6361/201323349
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI3AN
UT WOS:000336730900025
ER
PT J
AU Fremling, C
Sollerman, J
Taddia, F
Ergon, M
Valenti, S
Arcavi, I
Ben-Ami, S
Cao, Y
Cenko, SB
Filippenko, AV
Gal-Yam, A
Howell, DA
AF Fremling, C.
Sollerman, J.
Taddia, F.
Ergon, M.
Valenti, S.
Arcavi, I.
Ben-Ami, S.
Cao, Y.
Cenko, S. B.
Filippenko, A. V.
Gal-Yam, A.
Howell, D. A.
TI The rise and fall of the Type Ib supernova iPTF13bvn Not a massive
Wolf-Rayet star
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE supernovae: general; supernovae: individual: iPTF13bvn
ID CORE-COLLAPSE SUPERNOVA; LIGHT CURVES; LOW-RESOLUTION; X-RAY; EVOLUTION;
PROGENITOR; TELESCOPE; SPECTRA; I.; NUCLEOSYNTHESIS
AB Context. We investigate iPTF13bvn, a core-collapse (CC) supernova (SN) in the nearby spiral galaxy NGC 5806. This object was discovered by the intermediate Palomar Transient Factory (iPTF) very close to the estimated explosion date and was classified as a stripped-envelope CC SN, likely of Type Ib. Furthermore, a possible progenitor detection in pre-explosion Hubble Space Telescope (HST) images was reported, making this the only SN Ib with such an identification. Based on the luminosity and color of the progenitor candidate, as well as on early-time spectra and photometry of the SN, it was argued that the progenitor candidate is consistent with a single, massive Wolf-Rayet (WR) star.
Aims. We aim to confirm the progenitor detection, to robustly classify the SN using additional spectroscopy, and to investigate if our follow-up photometric and spectroscopic data on iPTF13bvn are consistent with a single-star WR progenitor scenario.
Methods. We present a large set of observational data, consisting of multi-band light curves (UBVRI, g' r' i' z') and optical spectra. We perform standard spectral line analysis to track the evolution of the SN ejecta. We also construct a bolometric light curve and perform hydrodynamical calculations to model this light curve to constrain the synthesized radioactive nickel mass and the total ejecta mass of the SN. Late-time photometry is analyzed to constrain the amount of oxygen. Furthermore, image registration of pre- and post-explosion HST images is performed.
Results. Our HST astrometry confirms the location of the progenitor candidate of iPTF13bvn, and follow-up spectra securely classify this as a SN Ib. We use our hydrodynamical model to fit the observed bolometric light curve, estimating the total ejecta mass to be 1.9 M-circle dot and the radioactive nickel mass to be 0.05 M-circle dot. The model fit requires the nickel synthesized in the explosion to be highly mixed out in the ejecta. We also find that the late-time nebular r'-band luminosity is not consistent with predictions based on the expected oxygen nucleosynthesis in very massive stars.
Conclusions. We find that our bolometric light curve of iPTF13bvn is not consistent with the previously proposed single massive WR-star progenitor scenario. The total ejecta mass and, in particular, the late-time oxygen emission are both significantly lower than what would be expected from a single WR progenitor with a main-sequence mass of at least 30 M-circle dot.
C1 [Fremling, C.; Sollerman, J.; Taddia, F.; Ergon, M.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, S-10691 Stockholm, Sweden.
[Valenti, S.; Arcavi, I.; Howell, D. A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Valenti, S.; Howell, D. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Arcavi, I.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Ben-Ami, S.; Gal-Yam, A.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Cao, Y.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Fremling, C (reprint author), Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, S-10691 Stockholm, Sweden.
EM christoffer.fremling@astro.su.se
OI Sollerman, Jesper/0000-0003-1546-6615
FU Swedish Research Council; W. M. Keck Foundation; EU/FP7 via ERC
[307260]; Israeli Committee for planning and budgeting; ISF grant; GIF
grant; Minerva grant; Kimmel award; Christopher R. Redlich Fund; TABASGO
Foundation; NSF [AST-1211916]; NASA from the Space Telescope Science
Institute [AR-12623, AR-12850]; NASA [NAS 5-26555]
FX The Oskar Klein Centre is funded by the Swedish Research Council. This
work is partially based on observations made with the Nordic Optical
Telescope, operated by the Nordic Optical Telescope Scientific
Association at the Observatorio del Roque de los Muchachos, La Palma,
Spain, of the Instituto de Astrofisica de Canarias. The data presented
here were obtained in part with ALFOSC, which is provided by the
Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with
the University of Copenhagen and NOTSA. Some of the data 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 NASA; the observatory was made
possible by the generous financial support of the W. M. Keck Foundation.
A. G.-Y. is supported by the EU/FP7 via ERC grant 307260, "The Quantum
Universe" I-Core program by the Israeli Committee for planning and
budgeting, by ISF, GIF, and Minerva grants, and by the Kimmel award. A.
V. F.'s group at UC Berkeley has received generous financial assistance
from the Christopher R. Redlich Fund, the TABASGO Foundation, NSF grant
AST-1211916, and NASA grants AR-12623 and AR-12850 from the Space
Telescope Science Institute (which is operated by AURA, Inc., under NASA
contract NAS 5-26555). We extend our thanks to the following people for
their various contributions to this work: Shri Kulkarni, Mansi M.
Kasliwal, Ofer Yaron, Paul Vreeswijk, Daniel Perley, Joel Johansson,
Anders Jerkstrand, Kelsey Clubb, Ori Fox, Patrick Kelly, Barak Zackay,
Adam Waszczak, Donald O'Sullivan, and Thomas Augusteijn.
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SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2014
VL 565
AR A114
DI 10.1051/0004-6361/201423884
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI3AN
UT WOS:000336730900114
ER
PT J
AU Grinberg, V
Pottschmidt, K
Bock, M
Schmid, C
Nowak, MA
Uttley, P
Tomsick, JA
Rodriguez, J
Hell, N
Markowitz, A
Bodaghee, A
Bel, MC
Rothschild, RE
Wilms, J
AF Grinberg, V.
Pottschmidt, K.
Boeck, M.
Schmid, C.
Nowak, M. A.
Uttley, P.
Tomsick, J. A.
Rodriguez, J.
Hell, N.
Markowitz, A.
Bodaghee, A.
Bel, M. Cadolle
Rothschild, R. E.
Wilms, J.
TI Long term variability of Cygnus X-1 VI. Energy-resolved X-ray
variability 1999-2011
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: binaries; stars: individual: Cygnus X-1; binaries: close
ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE CANDIDATES; ACCRETION-EJECTION
INSTABILITY; QUASI-PERIODIC OSCILLATIONS; TIMING-EXPLORER OBSERVATION;
POWER SPECTRAL COMPONENTS; DEPENDENT TIME LAGS; HARD STATE; XMM-NEWTON;
SOFT STATE
AB We present the most extensive analysis of Fourier-based X-ray timing properties of the black hole binary Cygnus X-1 to date, based on 12 years of bi-weekly monitoring with RXTE from 1999 to 2011. Our aim is a comprehensive study of timing behavior across all spectral states, including the elusive transitions and extreme hard and soft states. We discuss the dependence of the timing properties on spectral shape and photon energy, and study correlations between Fourier-frequency dependent coherence and time lags with features in the power spectra. Our main results are: (a) The fractional rms in the 0.125-256 Hz range in different spectral states shows complex behavior that depends on the energy range considered. It reaches its maximum not in the hard state, but in the soft state in the Comptonized tail above 10 keV. (b) The shape of power spectra in hard and intermediate states and the normalization in the soft state are strongly energy dependent in the 2.1-15 keV range. This emphasizes the need for an energy-dependent treatment of power spectra and a careful consideration of energy- and mass-scaling when comparing the variability of different source types, e.g., black hole binaries and AGN. PSDs during extremely hard and extremely soft states can be easily confused for energies above similar to 5 keV in the 0.125-256 Hz range. (c) The coherence between energy bands drops during transitions from the intermediate into the soft state but recovers in the soft state. (d) The time lag spectra in soft and intermediate states show distinct features at frequencies related to the frequencies of the main variability components seen in the power spectra and show the same shift to higher frequencies as the source softens. Our results constitute a template for other sources and for physical models for the origin of the X-ray variability. In particular, we discuss how the timing properties of Cyg X-1 can be used to assess the evolution of variability with spectral shape in other black hole binaries. Our results suggest that none of the available theoretical models can explain the full complexity of X-ray timing behavior of Cyg X-1, although several ansatzes with different physical assumptions are promising.
C1 [Grinberg, V.; Schmid, C.; Markowitz, A.; Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany.
[Grinberg, V.; Nowak, M. A.] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA.
[Pottschmidt, K.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Boeck, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Uttley, P.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
[Tomsick, J. A.; Bodaghee, A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Rodriguez, J.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,UMR 7158,IRFU SAp, F-91191 Gif Sur Yvette, France.
[Hell, N.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Markowitz, A.; Rothschild, R. E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Bel, M. Cadolle] Univ Munich, D-85748 Garching, Germany.
RP Grinberg, V (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, Sternwartstr 7, D-96049 Bamberg, Germany.
EM victoria.grinberg@fau.de
RI Wilms, Joern/C-8116-2013;
OI Wilms, Joern/0000-0003-2065-5410; Rodriguez, Jerome/0000-0002-4151-4468
FU Bundesministerium fur Wirtschaft und Technologie under Deutsches Zentrum
fur Luft- und Raumfahrt grants [50 OR 1007, 50 OR 1113]; European
Commission [ITN 215212]; LLNL [DE-AC52-07NA27344]; NASA [SV3-73016,
NAS8-03060]; NASA/GSFC
FX This work has been partially funded by the Bundesministerium fur
Wirtschaft und Technologie under Deutsches Zentrum fur Luft- und
Raumfahrt grants 50 OR 1007 and 50 OR 1113 and by the European
Commission through ITN 215212 "Black Hole Universe". It was partially
completed by LLNL under contract DE-AC52-07NA27344, and is supported by
NASA grants to LLNL and NASA/GSFC. Support for this work was also
provided by NASA through the Smithsonian Astrophysical Observatory (SAO)
contract SV3-73016 to MIT for Support of the Chandra X-Ray Center (CXC)
and Science Instruments; CXC is operated by SAO for and on behalf of
NASA under contract NAS8-03060. We further acknowledge support from the
DFG Cluster of Excellence "Origin and Structure of the Universe" and are
grateful for the support by MCB through the Computational Center for
Particle and Astrophysics (C2PAP). This research has made use of NASA's
Astrophysics Data System Bibliographic Services. We thank John E. Davis
for the development of the slxfig module used to prepare all figures in
this work and Fritz-Walter Schwarm and Ingo Kreykenbohm for their work
on the Remeis computing cluster. This research made use of ISIS
functions (isisscripts) provided by ECAP/Remeis observatory and
MIT9. Without the hard work by Evan Smith to schedule the Cyg
X-1 so uniformly for more than a decade, this paper would not have been
possible. V.G. is grateful for the support through the ESAC faculty
grant program to support student attendance at the workshop
"Spectral/timing properties of accreting objects: from X-ray binaries to
AGN" that proved pivotal for the basic idea behind this research.
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SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2014
VL 565
AR A1
DI 10.1051/0004-6361/201322969
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI3AN
UT WOS:000336730900001
ER
PT J
AU Marshall, JP
Moro-Martin, A
Eiroa, C
Kennedy, G
Mora, A
Sibthorpe, B
Lestrade, JE
Maldonado, J
Sanz-Forcada, J
Wyatt, MC
Matthews, B
Horner, J
Montesinos, B
Bryden, G
del Burgo, C
Greaves, JS
Ivison, RJ
Meeus, G
Olofsson, G
Pilbratt, GL
White, GJ
AF Marshall, J. P.
Moro-Martin, A.
Eiroa, C.
Kennedy, G.
Mora, A.
Sibthorpe, B.
Lestrade, J-E
Maldonado, J.
Sanz-Forcada, J.
Wyatt, M. C.
Matthews, B.
Horner, J.
Montesinos, B.
Bryden, G.
del Burgo, C.
Greaves, J. S.
Ivison, R. J.
Meeus, G.
Olofsson, G.
Pilbratt, G. L.
White, G. J.
TI Correlations between the stellar, planetary, and debris components of
exoplanet systems observed by Herschel
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE infrared: stars; infrared: planetary systems; circumstellar matter;
planet-disk interactions
ID EXTRA-SOLAR PLANETS; ANGLO-AUSTRALIAN PLANET; EARTH-LIKE PLANETS; 47
URSAE-MAJORIS; M-CIRCLE-PLUS; HIGH-RESOLUTION SIMULATIONS; HOBBY-EBERLY
TELESCOPE; NEPTUNE-MASS PLANET; SUN-LIKE STARS; HARPS SEARCH
AB Context. Stars form surrounded by gas- and dust-rich protoplanetary discs. Generally, these discs dissipate over a few (3-10) Myr, leaving a faint tenuous debris disc composed of second-generation dust produced by the attrition of larger bodies formed in the protoplanetary disc. Giant planets detected in radial velocity and transit surveys of main-sequence stars also form within the protoplanetary disc, whilst super-Earths now detectable may form once the gas has dissipated. Our own solar system, with its eight planets and two debris belts, is a prime example of an end state of this process.
Aims. The Herschel DEBRIS, DUNES, and GI' programmes observed 37 exoplanet host stars within 25 pc at 70, 100, and 160 mu m with the sensitivity to detect far-infrared excess emission at flux density levels only an order of magnitude greater than that of the solar system's Edgeworth-Kuiper belt. Here we present an analysis of that sample, using it to more accurately determine the (possible) level of dust emission from these exoplanet host stars and thereafter determine the links between the various components of these exoplanetary systems through statistical analysis.
Methods. We have fitted the flux densities measured from recent Herschel observations with a simple two parameter (T-d, L-IR/L-*) black-body model (or to the 3 sigma upper limits at 100 mu m). From this uniform approach we calculated the fractional luminosity, radial extent and dust temperature. We then plotted the calculated dust luminosity or upper limits against the stellar properties, e.g. effective temperature, metallicity, and age, and identified correlations between these parameters.
Results. A total of eleven debris discs are identified around the 37 stars in the sample. An incidence of ten cool debris discs around the Sun-like exoplanet host stars (29 +/- 9%) is consistent with the detection rate found by DUNES (20.2 +/- 2.0%). For the debris disc systems, the dust temperatures range from 20 to 80 K, and fractional luminosities (L-IR/L-*) between 2.4 x10(-6) and 4.1 x10(-4). In the case of non-detections, we calculated typical 3 sigma upper limits to the dust fractional luminosities of a few x10(-6).
Conclusions. We recover the previously identified correlation between stellar metallicity and hot-Jupiter planets in our data set. We find a correlation between the increased presence of dust, lower planet masses, and lower stellar metallicities. This confirms the recently identified correlation between cold debris discs and low-mass planets in the context of planet formation by core accretion.
C1 [Marshall, J. P.; Eiroa, C.; Maldonado, J.; Meeus, G.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
[Marshall, J. P.; Horner, J.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Moro-Martin, A.] Ctr Astrobiol, Dept Astrophys, Madrid 28850, Spain.
[Moro-Martin, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kennedy, G.; Wyatt, M. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain.
[Sibthorpe, B.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands.
[Lestrade, J-E] CNRS, Observ Paris, F-75014 Paris, France.
[Maldonado, J.] INAF Observ Astron Palermo, I-90134 Palermo, Italy.
[Sanz-Forcada, J.; Montesinos, B.] CSIC, INTA, Ctr Astrobiol CAB, Dept Astrophys, Madrid 28691, Spain.
[Matthews, B.] Natl Res Council Canada, Herzberg Astron & Astrophys, Victoria, BC V9E 2E7, Canada.
[Matthews, B.] Univ Victoria, Victoria, BC V8W 3P6, Canada.
[Horner, J.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia.
[Horner, J.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia.
[Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[del Burgo, C.] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico.
[Greaves, J. S.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Olofsson, G.] Stockholm Univ, Dept Astron, AlbaNova linivers Ctr, S-10691 Stockholm, Sweden.
[Pilbratt, G. L.] ESTEC SRE SA, ESA Astrophys & Fundamental Phys Missions Div, NL-2201 AZ Noordwijk, Netherlands.
[White, G. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[White, G. J.] Rutherford Appleton Lab, Chilton OX11 0QX, Oxon, England.
RP Marshall, JP (reprint author), Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
EM jonathan.marshall@uam.es
RI Ivison, R./G-4450-2011; Sanz-Forcada, Jorge/C-3176-2017; Montesinos,
Benjamin/C-3493-2017;
OI Ivison, R./0000-0001-5118-1313; Sanz-Forcada, Jorge/0000-0002-1600-7835;
Montesinos, Benjamin/0000-0002-7982-2095; Marshall,
Jonathan/0000-0001-6208-1801; Horner, Jonti/0000-0002-1160-7970;
Kennedy, Grant/0000-0001-6831-7547
FU Spanish grant [AYA 2011-26202]; European Union through ERC [279973];
Spitzer grant OT1_amoromar_1
FX This research has made use of NASA's Astrophysics Data System
Bibliographic Services. This research has made use of the SIMBAD
database, operated at CDS; Strasbourg, France. This research has made
use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at
exoplanets.org, and the Extrasolar Planets Encyclopedia at
exoplanets.eu. J.P.M., CE., J.M. and B.M. are partially supported by
Spanish grant AYA 2011-26202. This work was supported by the European
Union through ERC grant number no. 279973 (GMK and MCW) and has been
partially supported by Spitzer grant OT1_amoromar_1 (AMM).
NR 170
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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 MAY
PY 2014
VL 565
AR A15
DI 10.1051/0004-6361/201323058
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI3AN
UT WOS:000336730900015
ER
PT J
AU Moehler, S
Dreizler, S
LeBlanc, F
Khalack, V
Michaud, G
Richer, J
Sweigart, AV
Grundahl, F
AF Moehler, S.
Dreizler, S.
LeBlanc, F.
Khalack, V.
Michaud, G.
Richer, J.
Sweigart, A. V.
Grundahl, F.
TI Hot horizontal branch stars in NGC288-effects of diffusion and
stratification on their atmospheric parameters
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: horizontal-branch; stars: atmospheres; techniques: spectroscopic;
globular clusters: individual: NGC 288
ID GLOBULAR-CLUSTER M13; ABUNDANCE ANOMALIES; PHYSICAL PARAMETERS; MULTIPLE
POPULATIONS; HB STARS; VERTICAL STRATIFICATION; RADIATIVE LEVITATION;
B-STARS; NGC 288; CONSEQUENCES
AB Context. NGC288 is a globular cluster with a well-developed blue horizontal branch (HB) covering the u-jump that indicates the onset of diffusion. It is therefore well suited to study the effects of diffusion in blue HB stars.
Aims. We compare observed abundances with predictions from stellar evolution models calculated with diffusion and from stratified atmospheric models. We verify the effect of using stratified model spectra to derive atmospheric parameters. In addition, we investigate the nature of the overluminous blue HB stars around the u-jump.
Methods. We defined a new photometric index sz from uvby measurements that is gravity-sensitive between 8000 K and 12 000 K. Using medium-resolution spectra and Stromgren photometry, we determined atmospheric parameters (T-eff, log g) and abundances for the blue HB stars. We used both homogeneous and stratified model spectra for our spectroscopic analyses.
Results. The atmospheric parameters and masses of the hot HB stars in NGC288 show a behaviour seen also in other clusters for temperatures between 9000 K and 14 000 K. Outside this temperature range, however, they instead follow the results found for such stars in.Cen. The abundances derived from our observations are for most elements (except He and P) within the abundance range expected from evolutionary models that include the effects of atomic diffusion and assume a surface mixed mass of 10(-7) M-circle dot. The abundances predicted by stratified model atmospheres are generally significantly more extreme than observed, except for Mg. When effective temperatures, surface gravities, and masses are determined with stratified model spectra, the hotter stars agree better with canonical evolutionary predictions.
Conclusions. Our results show definite promise towards solving the long-standing problem of surface gravity and mass discrepancies for hot HB stars, but much work is still needed to arrive at a self-consistent solution.
C1 [Moehler, S.] European So Observ, D-85748 Garching, Germany.
[Moehler, S.] Inst Theoret Phys & Astrophys, D-24118 Kiel, Germany.
[Dreizler, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[LeBlanc, F.; Khalack, V.] Univ Moncton, Dept Phys & Astron, Moncton, NB E1A 3E9, Canada.
[Michaud, G.; Richer, J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Sweigart, A. V.] NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA.
[Grundahl, F.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
RP Moehler, S (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM smoehler@eso.org; dreizler@astro.physik.uni-goettingen.de;
francis.leblanc@umoncton.ca; viktor.khalak@umoncton.ca;
michaudg@umontreal.ca; jacques.richer@umontreal.ca;
allen.sweigart@gmail.com; fgj@phys.au.dk
OI Moehler, Sabine/0000-0002-4152-9643
NR 52
TC 5
Z9 5
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2014
VL 565
AR A100
DI 10.1051/0004-6361/201322953
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI3AN
UT WOS:000336730900100
ER
PT J
AU Presotto, V
Girardi, M
Nonino, M
Mercurio, A
Grillo, C
Rosati, P
Biviano, A
Annunziatella, M
Balestra, I
Cui, W
Sartoris, B
Lemze, D
Ascaso, B
Moustakas, J
Ford, H
Fritz, A
Czoske, O
Ettori, S
Kuchner, U
Lombardi, M
Maier, C
Medezinski, E
Molino, A
Scodeggio, M
Strazzullo, V
Tozzi, P
Ziegler, B
Bartelmann, M
Benitez, N
Bradley, L
Brescia, M
Broadhurst, T
Coe, D
Donahue, M
Gobat, R
Graves, G
Kelson, D
Koekemoer, A
Melchior, P
Meneghetti, M
Merten, J
Moustakas, LA
Munari, E
Postman, M
Regos, E
Seitz, S
Umetsu, K
Zheng, W
Zitrin, A
AF Presotto, V.
Girardi, M.
Nonino, M.
Mercurio, A.
Grillo, C.
Rosati, P.
Biviano, A.
Annunziatella, M.
Balestra, I.
Cui, W.
Sartoris, B.
Lemze, D.
Ascaso, B.
Moustakas, J.
Ford, H.
Fritz, A.
Czoske, O.
Ettori, S.
Kuchner, U.
Lombardi, M.
Maier, C.
Medezinski, E.
Molino, A.
Scodeggio, M.
Strazzullo, V.
Tozzi, P.
Ziegler, B.
Bartelmann, M.
Benitez, N.
Bradley, L.
Brescia, M.
Broadhurst, T.
Coe, D.
Donahue, M.
Gobat, R.
Graves, G.
Kelson, D.
Koekemoer, A.
Melchior, P.
Meneghetti, M.
Merten, J.
Moustakas, L. A.
Munari, E.
Postman, M.
Regos, E.
Seitz, S.
Umetsu, K.
Zheng, W.
Zitrin, A.
TI Intracluster light properties in the CLASH-VLT cluster MACS J1206.2-0847
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: clusters: individual: MACS J1206.2-0847; cosmology:
observations
ID DIFFUSE OPTICAL LIGHT; SIMULATED GALAXY CLUSTERS; STAR-FORMATION
EFFICIENCY; RAY BRIGHTEST CLUSTERS; X-RAY; SURFACE PHOTOMETRY; MASSIVE
GALAXIES; CD-GALAXIES; COSMOLOGICAL SIMULATIONS; DYNAMICAL FRICTION
AB Aims. We aim constrain the assembly history of clusters by studying the intracluster light (ICL) properties, estimating its contribution to the fraction of baryons in stars, f(*), and understanding possible systematics or bias using different ICL detection techniques.
Methods. We developed an automated method, GALtoICL, based on the software GALAPAGOS, to obtain a refined version of typical BCG+ICL maps. We applied this method to our test case MACS J1206.2-0847, a massive cluster located at z similar to 0 : 44, which is part of the CLASH sample. Using deep multiband Subaru images, we extracted the surface brightness (SB) profile of the BCG+ICL and studied the ICL morphology, color, and contribution to f(*) out to R500. We repeated the same analysis using a different definition of the ICL, SBlimit method, i.e., a SB cut-off level, to compare the results.
Results. The most peculiar feature of the ICL in MACS1206 is its asymmetric radial distribution, with an excess in the SE direction and extending toward the second brightest cluster galaxy, which is a post starburst galaxy. This suggests an interaction between the BCG and this galaxy that dates back to tau <= 1.5 Gyr. The BCG+ICL stellar content is similar to 8% of M-*, (500), and the (de-) projected baryon fraction in stars is f(*) = 0.0177(0.0116), in excellent agreement with recent results. The SBlimit method provides systematically higher ICL fractions and this effect is stronger at lower SB limits. This is due to the light from the outer envelopes of member galaxies that contaminate the ICL. Though more time consuming, the GALtoICL method provides safer ICL detections that are almost free of this contamination. This is one of the few ICL study at redshift z > 0.3. At completion, the CLASH/VLT program will allow us to extend this analysis to a statistically significant cluster sample spanning a wide redshift range: 0.2 less than or similar to z.0 less than or similar to 6.
C1 [Presotto, V.; Girardi, M.; Annunziatella, M.; Cui, W.; Sartoris, B.] Univ Trieste, Dipartimento Fis, I-34143 Trieste, Italy.
[Presotto, V.; Girardi, M.; Nonino, M.; Biviano, A.; Annunziatella, M.; Balestra, I.; Cui, W.; Sartoris, B.; Munari, E.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy.
[Mercurio, A.; Balestra, I.; Brescia, M.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Grillo, C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Rosati, P.] Univ Ferrara, Dipartimento Fis Sci Terra, I-44122 Ferrara, Italy.
[Cui, W.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia.
[Sartoris, B.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Lemze, D.; Ford, H.; Zheng, W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ascaso, B.; Molino, A.; Benitez, N.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA.
[Fritz, A.; Scodeggio, M.] IASF Milano, INAF, I-20133 Milan, Italy.
[Czoske, O.; Kuchner, U.; Maier, C.; Ziegler, B.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria.
[Ettori, S.; Meneghetti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Ettori, S.; Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy.
[Lombardi, M.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy.
[Medezinski, E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Strazzullo, V.] CEA Saclay, F-91191 Gif Sur Yvette, France.
[Tozzi, P.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Bartelmann, M.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany.
[Bradley, L.; Coe, D.; Koekemoer, A.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Broadhurst, T.] Univ Basque Country, Dept Theoret Phys, Bilbao 48080, Spain.
[Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Gobat, R.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM Paris Saclay,CEA,DSM,CNRS,Irfu, F-91191 Gif Sur Yvette, France.
[Graves, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Graves, G.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Melchior, P.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Merten, J.; Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Regos, E.] CERN, European Lab Particle Phys, CH-1211 Geneva 23, Switzerland.
[Seitz, S.] Univ Observ Munich, D-81679 Munich, Germany.
[Seitz, S.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Zitrin, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RP Presotto, V (reprint author), Univ Trieste, Dipartimento Fis, Via Tiepolo 11, I-34143 Trieste, Italy.
RI Ettori, Stefano/N-5004-2015; Grillo, Claudio/E-6223-2015; Meneghetti,
Massimo/O-8139-2015; Cui, Weiguang/P-4953-2014;
OI Biviano, Andrea/0000-0002-0857-0732; LOMBARDI,
MARCO/0000-0002-3336-4965; Moustakas, Leonidas/0000-0003-3030-2360;
Koekemoer, Anton/0000-0002-6610-2048; Benitez,
Narciso/0000-0002-0403-7455; Tozzi, Paolo/0000-0003-3096-9966; Ettori,
Stefano/0000-0003-4117-8617; Grillo, Claudio/0000-0002-5926-7143;
Meneghetti, Massimo/0000-0003-1225-7084; Cui,
Weiguang/0000-0002-2113-4863; Maier, Christian/0000-0001-6405-2182;
Nonino, Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X;
Scodeggio, Marco/0000-0002-2282-5850; Brescia,
Massimo/0000-0001-9506-5680; Umetsu, Keiichi/0000-0002-7196-4822
FU PRIN-INAF2010; MIUR [J91J12000450001]; European Commission's Framework
Programme 7, through the Marie Curie Initial Training Network CosmoComp
[PITN-GA-2009-238356]; ARC [DP130100117]; Survey Simulation Pipeline
(SSimPL); INAF through VIPERS; NASA [HST-HF-51334.01-A]; STScI
FX We thank the anonymous referee for constructive comments that helped us
to improve the manuscript. V.P. is grateful to Monaco, P., Murante, G.,
and De Grandi, S. for useful discussion and comments. V.P. acknowledges
the grant "Cofinanziamento di Ateneo 2010" and financial support from
PRIN-INAF2010 and MIUR PRIN2010-2011 (J91J12000450001). W.C.
acknowledges a fellowship from the European Commission's Framework
Programme 7, through the Marie Curie Initial Training Network CosmoComp
(PITN-GA-2009-238356), supports from ARC DP130100117 and from the Survey
Simulation Pipeline (SSimPL; http://ssimpl-universe.tk/). A.F.
acknowledges the support by INAF through VIPERS grants PRIN 2008 and
PRIN 2010. The work of LAM was carried out at Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. Support
for A.Z. is provided by NASA through Hubble Fellowship grant
#HST-HF-51334.01-A awarded by STScI.
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FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2014
VL 565
AR A126
DI 10.1051/0004-6361/201323251
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI3AN
UT WOS:000336730900126
ER
PT J
AU Reindl, N
Rauch, T
Parthasarathy, M
Werner, K
Kruk, JW
Hamann, WR
Sander, A
Todt, H
AF Reindl, N.
Rauch, T.
Parthasarathy, M.
Werner, K.
Kruk, J. W.
Hamann, W-R
Sander, A.
Todt, H.
TI The rapid evolution of the exciting star of the Stingray nebula
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: abundances; stars: evolution; stars: AGB and post-AGB; stars:
individual: SAO 244567; stars: fundamental parameters; planetary
nebulae: individual: Stingray nebula (Henize 3-1357)
ID INTERMEDIATE-MASS STARS; POST-AGB STARS; PLANETARY-NEBULA; STELLAR
EVOLUTION; SAKURAIS OBJECT; FG SAGITTAE; SAO-244567; TEMPERATURE;
ATMOSPHERES; EXTINCTION
AB Context. SAO 244567, the exciting star of the Stingray nebula, is rapidly evolving. Previous analyses suggested that it has heated up from an effective temperature of about 21 kK in 1971 to over 50 kK in the 1990s. Canonical post-asymptotic giant branch evolution suggests a relatively high mass while previous analyses indicate a low-mass star.
Aims. A comprehensive model-atmosphere analysis of UV and optical spectra taken during 1988-2006 should reveal the detailed temporal evolution of its atmospheric parameters and provide explanations for the unusually fast evolution.
Methods. Fitting line profiles from static and expanding non-LTE model atmospheres to the observed spectra allowed us to study the temporal change of effective temperature, surface gravity, mass-loss rate, and terminal wind velocity. In addition, we determined the chemical composition of the atmosphere.
Results. We find that the central star has steadily increased its effective temperature from 38 kK in 1988 to a peak value of 60 kK in 2002. During the same time, the star was contracting, as concluded from an increase in surface gravity from log g = 4.8 to 6.0 and a drop in luminosity. Simultaneously, the mass-loss rate declined from log(M/M-circle dot yr(-1)) = -9.0 to -11.6 and the terminal wind velocity increased from v(infinity) = 1800 km s(-1) to 2800 km s(-1). Since around 2002, the star stopped heating and has cooled down again to 55 kK by 2006. It has a largely solar surface composition with the exception of slightly subsolar carbon, phosphorus, and sulfur. The results are discussed by considering different evolutionary scenarios.
Conclusions. The position of SAO 244567 in the log T-eff-log g plane places the star in the region of sdO stars. By comparison with stellar-evolution calculations, we confirm that SAO 244567 must be a low-mass star (M < 0.55 M-circle dot). However, the slow evolution of the respective stellar evolutionary models is in strong contrast to the observed fast evolution and the young planetary nebula with a kinematical age of only about 1000 years. We speculate that the star could be a late He-shell flash object. Alternatively, it could be the outcome of close-binary evolution. Then SAD 244567 would be a low-mass (0.354 M-circle dot) helium pre-white dwarf after the common-envelope phase, during which the planetary nebula was ejected.
C1 [Reindl, N.; Rauch, T.; Werner, K.] Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany.
[Parthasarathy, M.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hamann, W-R; Sander, A.; Todt, H.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
RP Reindl, N (reprint author), Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, Sand 1, D-72076 Tubingen, Germany.
EM reindl@astro.uni-tuebingen.de
FU German Research Foundation (DFG) [WE 1312/41-1]; German Aerospace Center
(DLR) [05 OR 0806]; NASA [NAS5-26555]; NASA Office of Space Science
[NNX13AC07G]
FX N.R. is supported by the German Research Foundation (DFG, grant WE
1312/41-1), TR by the German Aerospace Center (DLR, grant 05 OR 0806).
We thank Marcelo Miguel Miller Bertolami and Philip Hall for helpful
discussions and comments. M.P. is grateful to Profs. Ajit K. Kembhavi,
Kandaswamy Subramanian and T. Padmanabhan for their kind encouragement,
support, and hospitality. This research has made use of the SIMBAD
database, operated at the CDS, Strasbourg, France. This research made
use of NASA's Astrophysics Data System. This work used the
profile-fitting procedure OWENS developed by M. Lemoine and the French
FUSE Team. 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 NNX13AC07G and by other
grants and contracts.
NR 49
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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 MAY
PY 2014
VL 565
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DI 10.1051/0004-6361/201323189
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI3AN
UT WOS:000336730900040
ER
PT J
AU Sanna, A
Cesaroni, R
Moscadelli, L
Zhang, Q
Menten, KM
Molinari, S
Garatti, ACO
De Buizer, JM
AF Sanna, A.
Cesaroni, R.
Moscadelli, L.
Zhang, Q.
Menten, K. M.
Molinari, S.
Garatti, A. Caratti O.
De Buizer, J. M.
TI A subarcsecond study of the hot molecular core in G023.01-00.41
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: kinematics and dynamics; instrumentation: high angular resolution;
stars individual: G23.01-0.41; stars: formation
ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; GALACTIC PLANE; MASSIVE
STARS; HI-GAL; OUTFLOWS; EMISSION; G23.01-0.41; PROTOSTARS; ACCRETION
AB Context. Searching for disk-outflow systems in massive star-forming regions is a key to assessing the main physical processes in the recipe of massive star formation.
Aims. We have selected a hot molecular core (HMC) in the high-mass star-forming region G023.011-00.41, where VLBI multi-epoch observations of water and methanol masers have suggested the existence of rotation and expansion within 2000 AU of its center. Our piu-pose is to image the thermal line and continuum emission at millimeter was to establish the physical parameters and velocity field of the gas in the region.
Methods. We performed SMA observations at 1.3 mm with both the most extended and compact array configurations, providing subarcsecond and high sensitivity maps of various molecular lines, including both hot-core and outflow tracers. We also reconstructed the spectral energy distribution of the region from millimeter to near infrared wavelengths, using the Herschel/Hi-GAL maps, as well as archival data.
Results. From the spectral energy distribution, we derive a bolometric luminosity of similar to 4 x 10(4) L-circle dot. Our interferometric observations reveal that the distribution of dense gas and dust in the HMC is significantly flattened and extends up to a radius of 8000 AU from the center of radio continuum and maser emission in the region. The equatorial plane of this HMC is strictly perpendicular to the elongation of the collimated bipolar outflow, as imaged on scales of similar to 0.1-0.5 pc in the main CO isotopomers, as well as in the SiO(5-4) line. In the innermost LIMC regions (less than or similar to 1000 AU), the velocity.field traced by the CH3CN (12(K)-11(K)) line emission shows that molecular gas is both expanding along the outflow direction following a Hubble law and rotating about the outflow axis, in agreement with the (3D) velocity field traced by methanol masers. The velocity field associated with rotation indicates a dynamical mass of similar to 19 M-circle dot at the center of the core. The latter is likely to be concentrated in a single O9.5 ZAMS star, consistent with the estimated bolometric luminosity of G023.01-00.41. The physical properties of the CO (2-1) outflow emission, such as its momentum rate 6 x 10(-3) M-circle dot km s(-1) yr(-1) and its outflow rate 2 x 10(-4) M circle dot yr(-1), support our estimates of the luminosity (and mass) of the embedded young stellar object.
C1 [Sanna, A.; Menten, K. M.; Garatti, A. Caratti O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Cesaroni, R.; Moscadelli, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Molinari, S.] INAF IFSI, I-00133 Rome, Italy.
[De Buizer, J. M.] NASA, Stratospher Observ Infrared Astron USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Sanna, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM asanna@mpifr-bonn.mpg.de
RI Molinari, Sergio/O-4095-2016;
OI Molinari, Sergio/0000-0002-9826-7525; Moscadelli,
Luca/0000-0002-8517-8881; Cesaroni, Riccardo/0000-0002-2430-5103;
Caratti o Garatti, Alessio/0000-0001-8876-6614; Zhang,
Qizhou/0000-0003-2384-6589
FU European Research Council for the ERC Advanced [247078]; National
Aeronautics and Space Administration
FX Comments from the anonymous referee, which helped improving our paper,
are gratefully acknowledged. Financial support by the European Research
Council for the ERC Advanced Grant GLOSTAR (ERC-2009-AdG, Grant
Agreement no. 247078) is gratefully acknowledged. This research made use
of the myXCLASS program
(https//www.astro.uni-koeln.de/projects/schilke/XCLASS), which accesses
the CDMS (http//www.cdms.de) and JPL (http://spec.jpl.nasa.gov)
molecular databases. This publication makes use of data products from
the Widefield 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.
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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 MAY
PY 2014
VL 565
AR A34
DI 10.1051/0004-6361/201323129
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI3AN
UT WOS:000336730900034
ER
PT J
AU Sokolovsky, KV
Schinzel, FK
Tanaka, YT
Abolmasov, PK
Angelakis, E
Bulgarelli, A
Carrasco, L
Cenko, SB
Cheung, CC
Clubb, KI
D'Ammando, F
Escande, L
Fegan, SJ
Filippenko, AV
Finke, JD
Fuhrmann, L
Fukazawa, Y
Hays, E
Healey, SE
Ikejiri, Y
Itoh, R
Kawabata, KS
Komatsu, T
Kovalev, YA
Kovalev, YY
Krichbaum, TP
Larsson, S
Lister, ML
Lott, B
Max-Moerbeck, W
Nestoras, I
Pittori, C
Pursimo, T
Pushkarev, AB
Readhead, ACS
Recillas, E
Richards, JL
Riquelme, D
Romani, RW
Sakimoto, K
Sasada, M
Schmidt, R
Shaw, MS
Sievers, A
Thompson, DJ
Uemura, M
Ungerechts, H
Vercellone, S
Verrecchia, F
Yamanaka, M
Yoshida, M
Zensus, JA
AF Sokolovsky, K. V.
Schinzel, F. K.
Tanaka, Y. T.
Abolmasov, P. K.
Angelakis, E.
Bulgarelli, A.
Carrasco, L.
Cenko, S. B.
Cheung, C. C.
Clubb, K. I.
D'Ammando, F.
Escande, L.
Fegan, S. J.
Filippenko, A. V.
Finke, J. D.
Fuhrmann, L.
Fukazawa, Y.
Hays, E.
Healey, S. E.
Ikejiri, Y.
Itoh, R.
Kawabata, K. S.
Komatsu, T.
Kovalev, Yu A.
Kovalev, Y. Y.
Krichbaum, T. P.
Larsson, S.
Lister, M. L.
Lott, B.
Max-Moerbeck, W.
Nestoras, I.
Pittori, C.
Pursimo, T.
Pushkarev, A. B.
Readhead, A. C. S.
Recillas, E.
Richards, J. L.
Riquelme, D.
Romani, R. W.
Sakimoto, K.
Sasada, M.
Schmidt, R.
Shaw, M. S.
Sievers, A.
Thompson, D. J.
Uemura, M.
Ungerechts, H.
Vercellone, S.
Verrecchia, F.
Yamanaka, M.
Yoshida, M.
Zensus, J. A.
TI Two active states of the narrow-line gamma-ray-loud AGN GB 1310+487
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE quasars: individual: GB 1310+487; galaxies: jets; gamma rays: galaxies;
radiation mechanisms: non-thermal; galaxies: active
ID LARGE-AREA TELESCOPE; BL-LACERTAE OBJECTS; SWIFT ULTRAVIOLET/OPTICAL
TELESCOPE; ALL-SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS;
INVERSE-COMPTON CATASTROPHE; COMPACT NONTHERMAL SOURCES; FERMI-DETECTED
BLAZARS; RAPID TEV VARIABILITY; AGILE SPACE MISSION
AB Context. Previously unremarkable, the extragalactic radio source GB 1310+487 showed gamma-ray flare on 2009 November 18, reaching a daily flux of similar to 10(-6) photons cm(-2) s(-1) at energies E > 100 MeV and became one of the brightest GeV sources for about two weeks. Its optical spectrum shows strong forbidden-line emission while lacking broad permitted lines, which is not typical for a blazar. Instead, the spectrum resembles those of narrow emission-line galaxies.
Aims. We investigate changes in the object's radio-to-GeV spectral energy distribution (SED) during and after the prominent gamma-ray flare with the aim of determining the nature of the object and of constraining the origin of the variable high-energy emission.
Methods. The data collected by the Fermi and AGILE satellites at gamma-ray energies; Swift at X-ray and ultraviolet (UV); the Kanata, NOT, and Keck telescopes at optical; OAGH and WISE at infrared (IR); and IRAM 30m, OVRO 40m, Effelsberg 100 m, RATAN-600, and VLBA at radio are analyzed together to trace the SED evolution on timescales of months.
Results. The gamma-ray/ radio-loud narrow-line active galactic nucleus (AGN) is located at redshift z = 0.638. It shines through an unrelated foreground galaxy at z = 0.500. The AGN light is probably amplified by gravitational lensing. The AGN SED shows a two-humped structure typical of blazars and gamma-ray-loud narrow-line Seyfert 1 galaxies, with the high-energy (inverse-Compton) emission dominating by more than an order of magnitude over the low-energy (synchrotron) emission during gamma-ray flares. The difference between the two SED humps is smaller during the low-activity state. Fermi observations reveal a strong correlation between the gamma-ray flux and spectral index, with the hardest spectrum observed during the brightest gamma-ray state. The gamma-ray flares occurred before and during a slow rising trend in the radio, but no direct association between gamma-ray and radio flares could be established.
Conclusions. If the gamma-ray flux is a mixture of synchrotron self-Compton and external Compton emission, the observed GeV spectral variability may result from varying relative contributions of these two emission components. This explanation fits the observed changes in the overall IR to gamma-ray SED.
C1 [Sokolovsky, K. V.; Schinzel, F. K.; Angelakis, E.; Fuhrmann, L.; Kovalev, Y. Y.; Krichbaum, T. P.; Nestoras, I.; Pushkarev, A. B.; Schmidt, R.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Sokolovsky, K. V.; Kovalev, Yu A.; Kovalev, Y. Y.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia.
[Sokolovsky, K. V.; Abolmasov, P. K.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Schinzel, F. K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
[Tanaka, Y. T.; Kawabata, K. S.; Uemura, M.; Yoshida, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Bulgarelli, A.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Carrasco, L.; Recillas, E.] Inst Nacl Astrofis Opt & Electr, Mexico City 72860, DF, Mexico.
[Cenko, S. B.; Clubb, K. I.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Cenko, S. B.; Hays, E.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Cheung, C. C.] Naval Res Lab, Washington, DC 20375 USA.
[D'Ammando, F.] Univ Perugia, Dipartimento Fis, I-060123 Perugia, Italy.
[D'Ammando, F.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[D'Ammando, F.] INAF IRA Bologna, I-40129 Bologna, Italy.
[Escande, L.] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France.
[Fegan, S. J.] Ecole Polytech, Lab Leprince Ringuet, CNRS, IN2P3, F-91120 Palaiseau, France.
[Finke, J. D.] US Naval Res Lab, Washington, DC 20375 USA.
[Fukazawa, Y.; Ikejiri, Y.; Itoh, R.; Komatsu, T.; Sakimoto, K.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Healey, S. E.; Romani, R. W.; Shaw, M. S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Larsson, S.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden.
[Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticie Phys, S-10691 Stockholm, Sweden.
[Larsson, S.] Stockholm Univ, Dept Phys, AlbaNova, S-10691 Stockholm, Sweden.
[Lister, M. L.; Richards, J. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Lott, B.] Univ Bordeaux, CENBG, UMR 5797, F-33170 Gradignan, France.
[Lott, B.] CNRS, CENBG, IN2P3, UMR 5797, F-33170 Gradignan, France.
[Max-Moerbeck, W.; Readhead, A. C. S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91101 USA.
[Pittori, C.; Verrecchia, F.] ASI ASDC, I-00044 Rome, Italy.
[Pursimo, T.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain.
[Pushkarev, A. B.] Pulkovo Observ, St Petersburg 196140, Russia.
[Pushkarev, A. B.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine.
[Riquelme, D.; Sievers, A.; Ungerechts, H.] Inst Radioastron Milimetr, Granada 18012, Spain.
[Sasada, M.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Vercellone, S.] INAF IASF Palermo, I-90146 Palermo, Italy.
[Yamanaka, M.] Kyoto Univ, Kwasan Observ, Yamashina Ku, Kyoto 6078471, Japan.
RP Sokolovsky, KV (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM kirx@scan.sai.msu.ru
RI Kovalev, Yuri/J-5671-2013; Sokolovsky, Kirill/D-2246-2015; Kovalev,
Yuri/N-1053-2015; Pushkarev, Alexander/M-9997-2015; Pittori,
Carlotta/C-7710-2016
OI Kovalev, Yuri/0000-0001-9303-3263; Sokolovsky,
Kirill/0000-0001-5991-6863; Pittori, Carlotta/0000-0001-6661-9779
FU INSU/CNRS (France); MPG (Germany); IGN (Spain); NASA [NNX08AW31G,
NNG06GG1G]; NSF [AST-0808050, AST-1211916]; NASA-Fermi [NNX08AV67G]; W.
M. Keck Foundation; NASA Fermi Guest Investigator program [NXX12A075G];
Russian Foundation for Basic Research [11-02-00368, 13-02-12103];
Physical Sciences Division of the Russian Academy of Sciences; Ministry
of Education and Science of the Russian Federation [8405,
14.518.11.7054]; Dynasty Foundation; Science Education Complex of the
Lebedev Physical Inst. (UNK-FIAN); Presidium of the Russian Academy of
Sciences; NASA/Fermi [NNX12AF12GA]; Christopher R. Redlich Fund; NASA
FX We thank Sara Cutini, Marco Ajello, Denis Bastieri, Boris Komberg, Seth
Digel, Luca Latronico and the anonymous referee for discussions and
comments that helped improve this paper. 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 (NASA) and the Department of Energy
in the United States, the Commissariat 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,
and the Swedish Research Council as well as 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. We acknowledge the use of public data from the Swift data
archive at the High Energy Astrophysics Science Archive Research Center
(HEASARC), provided by NASA's Goddard Space Flight Center. Based in part
on observations with the 100m telescope of the MPIfR
(Max-Planck-Institut fur Radioastronomie) and the IRAM 30m telescope.
IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).
The OVRO 40m monitoring program is supported in part by NASA grants
NNX08AW31G and NNG06GG1G, and by NSF grant AST-0808050. This research
has made use of data from the MOJAVE database that is maintained by the
MOJAVE team (Lister et al. 2009a). The data presented herein were
obtained in part with ALFOSC, which is provided by the Instituto de
Astrofisica de Andalucia (IAA) under a joint agreement with the
University of Copenhagen and NOTSA. The MOJAVE project is supported
under NASA-Fermi grant NNX08AV67G. Some of the data 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 NASA. The Observatory was made possible by
the generous financial support of the W. M. Keck Foundation. We thank O.
Fox, P. Kelly, I. Shivvers, and W. Zheng for assistance with some of the
Keck observations. The near-IR observations were carried out with the
2.1m telescope of the Guillermo Haro Observatory, INAOE, Mexico. F. K.
S. and K. V. S. were partly supported for this research. F. K. S.
acknowledges support by the NASA Fermi Guest Investigator program, grant
NXX12A075G. I.N. and R. S. are members of the International Max Planck
Research School (IMPRS) for Astronomy and Astrophysics at the
Universities of Bonn and Cologne. K. V. S., Y. A. K., and Y. Y. K. were
supported in part by the Russian Foundation for Basic Research (Projects
11-02-00368 and 13-02-12103), 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.; RATAN-600
operations were carried out with the financial support of the Ministry
of Education and Science of the Russian Federation (contract
14.518.11.7054). K. V. S. was supported by the Science Education Complex
of the Lebedev Physical Inst. (UNK-FIAN). A. B. P. was supported by the
"Non-stationary processes in the Universe" Program of the Presidium of
the Russian Academy of Sciences. A. V. F. and S. B. C. are grateful for
the support of NASA/Fermi grant NNX12AF12GA, NSF grant AST-1211916, the
Christopher R. Redlich Fund, and Gary and Cynthia Bengier. 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 NASA. We also used NASA's Astrophysics
Data System. K. V. S. thanks Maria Mogilen for her help in preparing
this manuscript.
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SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2014
VL 565
AR A26
DI 10.1051/0000-6361/201220703
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI3AN
UT WOS:000336730900026
ER
PT J
AU Ueta, T
Ladjal, D
Exter, KM
Otsuka, M
Szczerba, R
Siodmiak, N
Aleman, I
van Hoof, PAM
Kastner, JH
Montez, R
McDonald, I
Wittkowski, M
Sandin, C
Ramstedt, S
De Marco, O
Villaver, E
Chu, YH
Vlemmings, W
Izumiura, H
Sahai, R
Lopez, JA
Balick, B
Zijlstra, A
Tielens, AGGM
Rattray, RE
Behar, E
Blackman, EG
Hebden, K
Hora, JL
Murakawa, K
Nordhaus, J
Nordon, R
Yamamura, I
AF Ueta, T.
Ladjal, D.
Exter, K. M.
Otsuka, M.
Szczerba, R.
Siodmiak, N.
Aleman, I.
van Hoof, P. A. M.
Kastner, J. H.
Montez, R., Jr.
McDonald, I.
Wittkowski, M.
Sandin, C.
Ramstedt, S.
De Marco, O.
Villaver, E.
Chu, Y-H
Vlemmings, W.
Izumiura, H.
Sahai, R.
Lopez, J. A.
Balick, B.
Zijlstra, A.
Tielens, A. G. G. M.
Rattray, R. E.
Behar, E.
Blackman, E. G.
Hebden, K.
Hora, J. L.
Murakawa, K.
Nordhaus, J.
Nordon, R.
Yamamura, I.
TI The Herschel Planetary Nebula Survey (HerPlaNS) I. Data overview and
analysis demonstration with NGC 6781
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE infrared: stars; planetary nebulae: general; stars: winds, outflows;
stars: mass-loss; planetary nebulae: individual: NGC 6781; circumstellar
matter
ID GIANT BRANCH STARS; OPTICAL RECOMBINATION LINES; FAR-INFRARED
SPECTROSCOPY; INTERMEDIATE-MASS STARS; EXCITATION ATOMIC GAS;
HELIX-NEBULA; EVOLVED STARS; CHEMICAL ABUNDANCES; INTERSTELLAR-MEDIUM;
MAGELLANIC-CLOUD
AB Context. This is the first of a series of investigations into far-IR characteristics of 11 planetary nebulae (PNe) under the Herschel Space Observatory open time 1 program, Herschel Planetary Nebula Survey (HerPlaNS).
Aims. Using the HerPlaNS data set, we look into the PN energetics and variations of the physical conditions within the target nebulae. In the present work, we provide an overview of the survey, data acquisition and processing, and resulting data products.
Methods. We performed (1) PACS/SPIRE broadband imaging to determine the spatial distribution of the cold dust component in the target PNe and (2) PACS/SPIRE spectral-energy-distribution and line spectroscopy to determine the spatial distribution of the gas component in the target PNe.
Results. For the case of NGC 6781, the broadband maps confirm the nearly pole-on barrel structure of the amorphous carbon-rich dust shell and the surrounding halo having temperatures of 26-40 K. The PACS/SPIRE multiposition spectra show spatial variations of far-.IR lines that reflect the physical stratification of the nebula. We demonstrate that spatially resolved far-IR line diagnostics yield the (T-e, n(e)) profiles, from which distributions of ionized, atomic, and molecular gases can be determined. Direct comparison of the dust and gas column mass maps constrained by the HerPlaNS data allows to construct an empirical gas-to-dust mass ratio map, which shows a range of ratios with the median of 195 +/- 110. The present analysis yields estimates of the total mass of the shell to be 0.86 M-circle dot, consisting of 0.54 M-circle dot of ionized gas, 0.12 M-circle dot of atomic gas, 0.2 M-circle dot of molecular gas, and 4 x 10(-3) M-circle dot of dust grains. These estimates' also suggest that the central star of about 1.5 M-circle dot initial mass is terminating its PN evolution onto the white dwarf cooling track.
Conclusions. The HerPlaNS data provide various diagnostics for both the dust and gas components in a spatially resolved manner. In the forthcoming papers of the HerPlaNS series we will explore the HerPlaNS data set fully for the entire sample of 11 PNe.
C1 [Ueta, T.; Ladjal, D.; Rattray, R. E.] Univ Denver, Dept Phys & Astron, Denver, CO 80210 USA.
[Ueta, T.; Yamamura, I.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Exter, K. M.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Otsuka, M.] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan.
[Szczerba, R.; Siodmiak, N.] N Copernicus Astron Ctr, PL-87100 Torun, Poland.
[Aleman, I.; Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[van Hoof, P. A. M.] Royal Observ Belgium, B-1180 Brussels, Belgium.
[Kastner, J. H.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Montez, R., Jr.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[McDonald, I.; Zijlstra, A.; Hebden, K.] Jodrell Batik Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Wittkowski, M.] ESO, D-85748 Garching, Germany.
[Sandin, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
[Ramstedt, S.] Uppsala Univ, Div Astron & Space Phys, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[De Marco, O.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia.
[Villaver, E.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
[Chu, Y-H] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Vlemmings, W.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden.
[Izumiura, H.] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan.
[Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lopez, J. A.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 22800, Baja California, Mexico.
[Balick, B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Behar, E.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
[Blackman, E. G.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14618 USA.
[Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Murakawa, K.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Nordhaus, J.] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA.
[Nordon, R.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany.
RP Ueta, T (reprint author), Univ Denver, Dept Phys & Astron, 2112 E Wesley Ave, Denver, CO 80210 USA.
EM tueta@du.edu
RI Aleman, Isabel/F-3251-2012;
OI /0000-0002-2700-9916; Wittkowski, Markus/0000-0002-7952-9550
FU NASA by jet Propulsion Laboratory, Caltech; NASA by jet Propulsion
Laboratory, Ladjal; NASA by jet Propulsion Laboratory, Kastner; NASA by
jet Propulsion Laboratory, Sahai; Japan Society for the Promotion of
Science (JSPS); Belgian Federal Science Policy Office via the PRODEX
Programme of ESA; Polish NCN [2011/01/B/ST9/02031]; European Research
Council via the advanced-ERC [246976]; Dutch Science Agency (NWO) via
the Dutch Astrochemistry Network; NASA
FX This work is based on observations made with the Herschel Space
Observatory, a European Space Agency (ESA) Cornerstone Mission with
significant participation by NASA. Support for this work was provided by
NASA through an award issued by jet Propulsion Laboratory, Caltech
Ladjal, Kastner, Sahai), the Japan Society for the Promotion of Science
(JSPS) through a FY2013 long-term invitation fellowship program (Ueta),
the Belgian Federal Science Policy Office via the PRODEX Programme of
ESA (Exter, van Hoof), the Polish NCN through a grant
2011/01/B/ST9/02031 (Szczerba, Siodmiak), and the European Research
Council via the advanced-ERC grant 246976 and the Dutch Science Agency
(NWO) via the Dutch Astrochemistry Network and the Spinoza prize
(Aleman, Tielens). The authors thank M. A. Guerrero for sharing the NOT
optical images of NGC 6781 with us. Also, H. Monteiro's generosity is
appreciated for the reproduction of one of his figures (Fig. 3 of
Schwarz & Monteiro 2006). Sahai acknowledges that his contribution to
the research described here was carried out at the JPE/Caltech, under a
contract with NASA. Finally, Ueta also acknowledges the hospitality of
the members of the Laboratory of Infrared Astrophysics at ISAS/JAXA
during his sabbatical stay as a JSPS invitation fellow.
NR 84
TC 7
Z9 7
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2014
VL 565
AR A36
DI 10.1051/0004-6361/201423395
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI3AN
UT WOS:000336730900036
ER
PT J
AU Waizmann, JC
Redlich, M
Meneghetti, M
Bartelmann, M
AF Waizmann, J-C
Redlich, M.
Meneghetti, M.
Bartelmann, M.
TI The strongest gravitational lenses Ill. The order statistics of the
largest Einstein radii
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gravitational lensing: strong; methods: statistical; galaxies: clusters:
general; cosmology: miscellaneous
ID STRONG-LENSING ANALYSIS; MACS J0717.5+3745; GALAXY CLUSTERS; LAMBDA-CDM;
MASS-DISTRIBUTION; COMPLETE SAMPLE; ARC STATISTICS; UNIVERSE; IMAGES;
A1689
AB Context. The Einstein radius of a gravitational lens is a key characteristic. It encodes information about decisive quantities such as halo mass, concentration, triaxiality, and orientation with respect to the observer. Therefore, the largest Einstein radii can potentially be utilised to test the predictions of the ACDM model. Aims. Hitherto, studies have focussed on the single largest observed Einstein radius. We extend those studies by employing order statistics to formulate exclusion criteria based on the n largest Einstein radii and apply these criteria to the strong lensing analysis of 12 MACS clusters at z > 0.5.
Methods. We obtain the order statistics of Einstein radii by a Monte Carlo approach, based on the semi-analytic modelling of the halo population on the past lightcone. After sampling the order statistics, we fit a general extreme value distribution to the first-order distribution, which allows us to derive analytic relations for the order statistics of the Einstein radii.
Results. We find that the Einstein radii of the 12 MACS clusters are not in conflict with the ACDM expectations. Our exclusion criteria indicate that, in order to exhibit tension with the concordance model, one would need to observe approximately twenty Einstein radii with theta(eff) greater than or similar to 30 '', ten with theta(eff) greater than or similar to 35 '', five with theta(eff) greater than or similar to 42 '', or one with theta(eff) greater than or similar to 74 '' in the redshift range 0.5 <= z <= 1.0 on the full sky (assuming a source redshift of z(s) = 2). Furthermore, we find that, with increasing order, the haloes with the largest Einstein radii are on average less aligned along the line-of-sight and less triaxial. In general, the ctunulative distribution functions steepen for higher orders, giving them better constraining power.
Conclusions. A framework that allows the individual and joint order distributions of the n-largest Einstein radii to be derived is presented. From a statistical point of view, we do not see any evidence of an Einstein ring problem even for the largest Einstein radii of the studied MACS sample. This conclusion is consolidated by the large uncertainties that enter the lens modelling and to which the largest Einstein radii are particularly sensitive.
C1 [Waizmann, J-C] Blue Yonder GmbH, D-76139 Karlsruhe, Germany.
[Waizmann, J-C] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy.
[Waizmann, J-C; Meneghetti, M.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Waizmann, J-C; Meneghetti, M.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy.
[Redlich, M.; Bartelmann, M.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Meneghetti, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Waizmann, JC (reprint author), Blue Yonder GmbH, Karlsruher Str 88, D-76139 Karlsruhe, Germany.
EM jean-claude.waizmann@blue-yonder.com
RI Meneghetti, Massimo/O-8139-2015
OI Meneghetti, Massimo/0000-0003-1225-7084
FU ASI-INAF [I/023/05/0, I/088/06/0]; ASI [I/016/07/0 COFIS]; ASI
Euclid-DUNE [I/064/08/0]; ASI-Uni Bologna-Astronomy Dept. Euclid-NIS
[I/039/10/0]; PRIN MIUR; German Academic Exchange Service (DAAD);
Internationale Spitzenforschung II-1 of the Baden-Wurttemberg Stiftung;
Dark Universe of the German Science Foundation
[Transregio-Sonderforschungsbereich TR 33]
FX J.C.W. acknowledges financial contributions from the contracts ASI-INAF
I/023/05/0, ASI-INAF I/088/06/0, ASI I/016/07/0 COFIS, ASI Euclid-DUNE
I/064/08/0, ASI-Uni Bologna-Astronomy Dept. Euclid-NIS I/039/10/0, and
PRIN MIUR 2008 Dark energy and cosmology with large galaxy surveys. M.R.
thanks the Sydney Institute for Astronomy for the hospitality and the
German Academic Exchange Service (DAAD) for their financial support.
Furthermore, M.R.'s work was supported in part by contract research
Internationale Spitzenforschung II-1 of the Baden-Wurttemberg Stiftung.
M.B. is supported in part by the Transregio-Sonderforschungsbereich TR
33 The Dark Universe of the German Science Foundation.
NR 33
TC 3
Z9 3
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2014
VL 565
AR A28
DI 10.1051/0004-6361/201323022
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI3AN
UT WOS:000336730900028
ER
PT J
AU Li, C
Su, CH
Lehoczky, SL
Scripa, RN
Ban, H
Lin, B
AF Li, C.
Su, Ching-Hua
Lehoczky, S. L.
Scripa, R. N.
Ban, H.
Lin, B.
TI Thermophysical properties of HgTe and Hg0.9Cd0.1Te melts
SO JOURNAL OF NON-CRYSTALLINE SOLIDS
LA English
DT Article
DE II-VI semiconductor melt; Density; Electrical conductivity; Viscosity
ID ELECTRICAL-CONDUCTIVITY; DISORDERED MATERIALS; LIQUID TE; VISCOSITY;
HG1-XCDXTE; DENSITY; HG0.8CD0.2TE; TRANSPORT; MERCURY; PHASE
AB Thermophysical properties, namely, density, viscosity, and electrical conductivity of HgTe and Hg0.9Cd0.1Te melts were measured as a function of temperature. A pycnometric method was used to measure the melt density in the temperature range of 948 to 1073 K for the HgTe melt and 1011 to 1131 K for the Hg0.9Cd0.1Te melt. The density results show a maximum at 1023 and 1020 K, respectively, for the HgTe and Hg0.9Cd0.1Te melts. The viscosity and electrical conductivity were simultaneously determined using a transient torque method from 944 to 1098 K for the HgTe melt and from 1016 to 1127 K for the Hg0.9Cd0.1Te melt. The measured electrical conductivity decreases as the mole fraction of CdTe, x, increases at a specific temperature, and increases as a function of temperature, which shows a semiconductor-like behavior. The measured viscosity decreases as the mole fraction of CdTe, x, increases at a specific temperature and decreases as the temperature increased. The analysis of the electrical conductivity of the melts and the relationship between the kinematic viscosity and density implied a structural transition in these melts. No relaxation phenomena were observed in the density, electrical conductivity, and viscosity of the HgTe and Hg0.9Cd0.1Te melts. Published by Elsevier B.V.
C1 [Li, C.; Scripa, R. N.] Univ Alabama Birmingham, Dept Mat Sci & Engn, Birmingham, AL 35294 USA.
[Su, Ching-Hua; Lehoczky, S. L.] NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL 35812 USA.
[Ban, H.; Lin, B.] Univ Alabama Birmingham, Dept Mech Engn, Birmingham, AL 35294 USA.
RP Su, CH (reprint author), NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL 35812 USA.
EM ching.h.su@nasa.gov
FU Advanced Capabilities Division, Exploration Systems Mission Directorate,
NASA Headquarter
FX The author would like to acknowledge the supports of the Advanced
Capabilities Division, Exploration Systems Mission Directorate, NASA
Headquarter.
NR 26
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U1 1
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-3093
EI 1873-4812
J9 J NON-CRYST SOLIDS
JI J. Non-Cryst. Solids
PD MAY 1
PY 2014
VL 391
BP 54
EP 60
DI 10.1016/j.jnoncrysol.2014.03.012
PG 7
WC Materials Science, Ceramics; Materials Science, Multidisciplinary
SC Materials Science
GA AI5AA
UT WOS:000336876600010
ER
PT J
AU Agu, NC
Redwine, KM
Bell, C
Garcia, KM
Martin, DS
Poffenbarger, TS
Bricker, JT
Portman, RJ
Gupta-Malhotra, M
AF Agu, Ngozi C.
Redwine, Karen McNiece
Bell, Cynthia
Garcia, Kathleen Marie
Martin, David S.
Poffenbarger, Tim S.
Bricker, John T.
Portman, Ronald J.
Gupta-Malhotra, Monesha
TI Detection of early diastolic alterations by Tissue Doppler Imaging in
untreated childhood-onset essential hypertension
SO JOURNAL OF THE AMERICAN SOCIETY OF HYPERTENSION
LA English
DT Article
DE Echocardiography; hypertension; pediatrics; insulin; diastole
ID LEFT-VENTRICULAR MASS; ALTERED MYOCARDIAL-METABOLISM; MITRAL ANNULUS
VELOCITY; BLOOD-PRESSURE; CARDIOVASCULAR-DISEASE; DIABETES-MELLITUS;
AMERICAN-SOCIETY; HEART-FAILURE; BODY-SIZE; CHILDREN
AB The aim of the study was to determine the presence of preclinical diastolic dysfunction in hypertensive children relative to normotensive children by Tissue Doppler Imaging (TDI). We prospectively enrolled children with untreated essential hypertension in absence of any other disease and a matched healthy control group with normal blood pressure (BP); both groups confirmed by clinic BP and a 24-hour ambulatory BP monitoring. Echocardiographic diastolic parameters were determined using spectral transmitral inflow Doppler, flow propagation velocity, TDI, and systolic parameters were determined via midwall shortening fraction and ejection fraction. A total of 80 multiethnic children were prospectively enrolled for the study: 46 hypertensive (median age, 13 years; 72% males) and 34 control (median age, 14 years; 65% males). The only echocardiography parameters that had a statistically significant change compared with the control children, were regional mitral Ea, Aa, and the E/Ea ratio by TDI. In comparison with controls, hypertensive children had lower Ea and Aa velocities of anterior and posterior walls and higher lateral wall E/Ea ratio. The decrease in posterior wall Ea and Aa remained significant after adjustment for gender, age, body mass index, ethnicity, and left ventricular hypertrophy on multivariate analysis. The lateral and septal wall E/Ea ratios correlated significantly with fasting serum insulin levels on similar multivariate analysis. Decreased regional TDI velocities were seen with preserved left ventricular systolic function even when other measures of diastolic dysfunction remained unchanged in untreated hypertensive children. Hypertension and serum insulin levels had strong associations with preclinical diastolic alterations in children. (C) 2014 American Society of Hypertension. All rights reserved.
C1 [Agu, Ngozi C.; Bricker, John T.; Gupta-Malhotra, Monesha] Univ Texas Houston, Childrens Mem Hermann Hosp, Sch Med, Dept Pediat,Div Pediat Cardiol, Houston, TX 77030 USA.
[Redwine, Karen McNiece; Gupta-Malhotra, Monesha] Univ Arkansas Med Sci, Arkansas Childrens Hosp, Dept Pediat, Div Pediat Nephrol, Little Rock, AR 72205 USA.
[Redwine, Karen McNiece; Bell, Cynthia; Poffenbarger, Tim S.; Portman, Ronald J.] Univ Texas Houston, Childrens Mem Hermann Hosp, Sch Med, Dept Pediat,Div Pediat Nephrol, Houston, TX 77030 USA.
[Garcia, Kathleen Marie; Martin, David S.] Wyle Sci Technol & Engn, Natl Aeronaut & Space Adm, Johnson Space Ctr, Cardiovasc Lab, Houston, TX USA.
RP Gupta-Malhotra, M (reprint author), Univ Texas Houston, Childrens Mem Hermann Hosp, Houston Med Sch, Div Pediat Cardiol, 6410 Fannin St,UTPB Ste 425, Houston, TX 77030 USA.
EM Monesha.gupta@uth.tmc.edu
RI Bell, Cynthia/B-1634-2009
OI Bell, Cynthia/0000-0002-2366-1843
FU National Heart, Lung, and Blood Institute [K23HL089391]; Dr Gupta's
Faculty Development Grant - University of Texas Health Science Center at
Houston; Dr Redwine's Ruth L. Kirschstein National Research Service
Individual Fellowship Award [F32 HL079813]; University of Texas Health
Science Center at Houston General Clinical Research Center [M01-RR 0255]
FX The project described was partially supported by Grant Number
K23HL089391 (PI Monesha Gupta) from the National Heart, Lung, and Blood
Institute. The content is solely the responsibility of the authors and
does not necessarily represent the official views of the National Heart,
Lung, and Blood Institute or the National Institutes of Health. A
portion of the study was funded by Dr Gupta's Faculty Development Grant
from the University of Texas Health Science Center at Houston. A portion
of the study was funded by Dr Redwine's Ruth L. Kirschstein National
Research Service Individual Fellowship Award (F32 HL079813) and the
University of Texas Health Science Center at Houston General Clinical
Research Center (M01-RR 0255).
NR 51
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Z9 6
U1 0
U2 1
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1933-1711
EI 1878-7436
J9 J AM SOC HYPERTENS
JI J. Am. Soc. Hypertens.
PD MAY
PY 2014
VL 8
IS 5
BP 303
EP 311
DI 10.1016/j.jash.2014.02.008
PG 9
WC Peripheral Vascular Disease
SC Cardiovascular System & Cardiology
GA AI5DS
UT WOS:000336886200005
PM 24685005
ER
PT J
AU Davarian, F
AF Davarian, Faramaz
TI In Search of Earth-Like Planets
SO PROCEEDINGS OF THE IEEE
LA English
DT Editorial Material
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Davarian, F (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 1
TC 0
Z9 0
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9219
EI 1558-2256
J9 P IEEE
JI Proc. IEEE
PD MAY
PY 2014
VL 102
IS 5
SI SI
BP 643
EP 645
DI 10.1109/JPROC.2014.2314771
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA AI5NR
UT WOS:000336915700001
ER
PT J
AU Hartwig, J
Darr, S
AF Hartwig, Jason
Darr, Samuel
TI Influential factors for liquid acquisition device screen selection for
cryogenic propulsion systems
SO APPLIED THERMAL ENGINEERING
LA English
DT Article
DE Cryogenics; Liquid acquisition device; Porous screen; Surface tension;
Fuel depot
ID SURFACE-TENSION; POINT; MIXTURES; FLOW
AB This paper presents the influential factors which govern screen selection for liquid acquisition devices (LADS) operating in microgravity conditions for future in-space cryogenic propulsion engines and cryogenic propellant depots. Space flight requirements, which include mass flow rate, acceleration level and direction, and thermal environment, dictate screen selection for a particular mission. The five influential factors include bubble point pressure, flow-through-screen pressure drop, wicking rate, screen compliance, and material compatibility. Governing equations and analytical models for these parameters are developed from first principles. A comprehensive survey of the historical data on coarser LAD meshes over four decades of work is conducted, and liquid hydrogen data for finer Dutch Twill meshes (325 x 2300, 450 x 2750, 510 x 3600) from recently concluded experiments is also presented to validate analytical models. Each of these parameters is measurable from ground based tests, making it facile to predict flight system performance. Therefore analytical models in this paper will be valuable for future LAD designs for both cryogenic and storable propulsion systems. Additionally, analysis will be given on the impact of the factors on liquid hydrogen systems. Published by Elsevier Ltd.
C1 [Hartwig, Jason] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Darr, Samuel] Univ Florida, Gainesville, FL 32611 USA.
RP Hartwig, J (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Jason.W.Hartwig@nasa.gov
OI Darr, Samuel/0000-0002-1891-405X
NR 55
TC 12
Z9 13
U1 0
U2 6
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 MAY
PY 2014
VL 66
IS 1-2
BP 548
EP 562
DI 10.1016/j.applthermaleng.2014.02.022
PG 15
WC Thermodynamics; Energy & Fuels; Engineering, Mechanical; Mechanics
SC Thermodynamics; Energy & Fuels; Engineering; Mechanics
GA AH7YT
UT WOS:000336352000057
ER
PT J
AU Kolli, KK
Arif, I
Peelukhana, SV
Succop, P
Back, LH
Helmy, TA
Leesar, MA
Effat, MA
Banerjee, RK
AF Kolli, Kranthi K.
Arif, Imran
Peelukhana, Srikara V.
Succop, Paul
Back, Lloyd H.
Helmy, Tarek A.
Leesar, Massoud A.
Effat, Mohamed A.
Banerjee, Rupak K.
TI Diagnostic Performance of Pressure Drop Coefficient in Relation to
Fractional Flow Reserve and Coronary Flow Reserve
SO JOURNAL OF INVASIVE CARDIOLOGY
LA English
DT Article
DE coronary disease; FFR; CFR; catheterization; meta-analysis
ID CONCOMITANT MICROVASCULAR DISEASE; HEMODYNAMIC END-POINTS; PORCINE
MODEL; VELOCITY RESERVE; BLOOD-FLOW; CARDIAC-CATHETERIZATION;
ARTERY-DISEASE; HEART-RATE; STENOSIS; INDEX
AB Objectives and Background. Functional assessment of coronary lesion severity during cardiac catheterization is conducted using diagnostic parameters like fractional flow reserve (FFR; pressure derived) and coronary flow reserve (CFR; flow derived). However, the complex hemodynamics of stenosis might not be sufficiently explained by either pressure or flow alone, particularly in the case of intermediate stenosis. CDP (ratio of pressure drop across a stenosis to distal dynamic pressure), a non-dimensional index derived from fundamental fluid dynamic principles based on a combination of intracoronary pressure and flow, may improve the functional assessment of coronary lesion severity. Methods. We performed a meta-analysis of seven studies, retrieved from MEDLINE and PubMed, comparing the results of FFR and CFR of the same lesions. Two studies reported functional measurements (pressure and flow) obtained in individual patients. Five studies reported two-dimensional plots of FFR vs CFR. The FFR and CFR data were digitized and corresponding funetional measurements were extracted using the reported mean values of hemodynamic data from each of the five studies. The receiver operating characteristic (ROC) curve was used to identify the optimal cut-off point of CDP, which corresponds to the clinically used cut-off values (FFR = 0.80, FFR = 0.75, and CFR = 2.0). Results. CDP correlated significantly with FFR (r = 0.78; P<.001) and had significant diagnostic efficiency (area under the ROC curve = 89%), specificity (83% and 85%), and sensitivity (81% and 76%) at FFR <0.8 and FFR <0.75, respectively. The corresponding cut-off value for CDP to detect FFR <0.80 and FFR <0.75 was at CDP >27.1 and CDP >27.9, respectively. Conclusions. CDP, a functional parameter based on both intracoronary pressure and flow measurements, has close agreement (area under the ROC curve = 89%) with FFR, the most frequently used method for evaluation of coronary stenosis severity.
C1 [Kolli, Kranthi K.; Peelukhana, Srikara V.; Banerjee, Rupak K.] Univ Cincinnati, Dept Mech & Mat Engn, Cincinnati, OH USA.
[Arif, Imran; Helmy, Tarek A.; Effat, Mohamed A.] Univ Cincinnati, Div Cardiovasc Dis, Cincinnati, OH USA.
[Succop, Paul] Univ Cincinnati, Dept Environm Hlth, Cincinnati, OH USA.
[Kolli, Kranthi K.; Arif, Imran; Peelukhana, Srikara V.; Helmy, Tarek A.; Effat, Mohamed A.; Banerjee, Rupak K.] Vet Affairs Med Ctr, Cincinnati, OH 45267 USA.
[Back, Lloyd H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Leesar, Massoud A.] Univ Alabama Birmingham, Div Cardiovasc Dis, Birmingham, AL USA.
RP Banerjee, RK (reprint author), Dept Mech & Mat Engn, 598 Rhodes Hall,POB 210072, Cincinnati, OH 45221 USA.
EM Rupak.Banerjee@UC.edu
FU Department of Veteran Affairs through VA Merit Review Grant
[I01CX000342-01]
FX This work is supported by financial support from Department of Veteran
Affairs through VA Merit Review Grant (I01CX000342-01).
NR 36
TC 3
Z9 3
U1 1
U2 4
PU H M P COMMUNICATIONS
PI MALVERN
PA 83 GENERAL WARREN BLVD, STE 100, MALVERN, PA 19355 USA
SN 1042-3931
EI 1557-2501
J9 J INVASIVE CARDIOL
JI J. Invasive Cardiol.
PD MAY
PY 2014
VL 26
IS 5
BP 188
EP 195
PG 8
WC Cardiac & Cardiovascular Systems
SC Cardiovascular System & Cardiology
GA AI0BM
UT WOS:000336511200001
PM 24791716
ER
PT J
AU Fulton, JA
Edwards, JR
Hassan, HA
McDaniel, JC
Goyne, CP
Rockwell, RD
Cutler, AD
Johansen, CT
Danehy, PM
AF Fulton, Jesse A.
Edwards, Jack R.
Hassan, Hassan A.
McDaniel, James C.
Goyne, Christopher P.
Rockwell, Robert D.
Cutler, Andrew D.
Johansen, Craig T.
Danehy, Paul M.
TI Large-Eddy/Reynolds-Averaged Navier-Stokes Simulations of Reactive Flow
in Dual-Mode Scramjet Combustor
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
ID LARGE-EDDY SIMULATION; SUPERSONIC COMBUSTION; HYDROGEN-AIR
AB Numerical simulations of the turbulent reactive flow within a model scramjet combustor configuration, experimentally mapped at the University of Virginia's Scramjet Combustion Facility at an equivalence ratio of 0.17, are described in this paper. A hybrid large-eddy simulation/Reynolds-averaged Navier-Stokes method is used, with special attention focused on capturing facility-specific effects, such as asymmetric inflow temperature distributions, on flow development within the combustor. Predictions obtained using two nine-species hydrogen oxidation models are compared with experimental data obtained using coherent anti-Stokes Raman spectroscopy, hydroxyl radical planar laser-induced fluorescence, stereoscopic particle image velocimetry, and focusing schlieren techniques. The large-eddy simulation/Reynolds-averaged Navier-Stokes models accurately capture the mean structure of the fully developed flame but tend to overpredict fluctuation levels toward the outer edge of the reactive plume. Model predictions worsen in the flame-anchoring region just downstream of the fuel injector. Here, turbulence/chemistry interactions are more pronounced, and the flame is more influenced by the inflow conditions. Comparisons with hydroxyl radical planar laser-induced fluorescence imagery indicate that the large-eddy simulation/Reynolds-averaged Navier-Stokes model can capture the effects of larger turbulent scales in deforming the flame structure but does not capture the effects of small turbulent structures in broadening the OH profiles.
C1 [Fulton, Jesse A.; Edwards, Jack R.; Hassan, Hassan A.] N Carolina State Univ, Raleigh, NC 27695 USA.
[McDaniel, James C.; Goyne, Christopher P.; Rockwell, Robert D.] Univ Virginia, Charlottesville, VA 22904 USA.
[Cutler, Andrew D.] George Washington Univ, Newport News, VA 23602 USA.
[Johansen, Craig T.] Univ Calgary, Calgary, AB T2N 1N4, Canada.
[Danehy, Paul M.] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA.
RP Fulton, JA (reprint author), N Carolina State Univ, Raleigh, NC 27695 USA.
FU National Center for Hypersonic Combined Cycle Propulsion [FA
9550-09-1-0611]
FX This work was sponsored by the National Center for Hypersonic Combined
Cycle Propulsion (grant FA 9550-09-1-0611), with technical monitors
Chiping Li (U.S. Air Force Office of Scientific Research) and Rick
Gaffney (NASA). The authors would like to thank Chad Smith at the
University of Virginia; Gaetano Magnotti, Luca Cantu, and Emanuela Gallo
at George Washington University; Ron Hanson, Jay Jeffries, Ian Schultz,
and Chris Goldenstein at Stanford University; and Toshinori Kouchi at
Tohoku University for providing experimental data and for many helpful
discussions. Computing time was obtained from NASA's National Academy of
Science supercomputing resource and by the Department,of Defense's
High-Performance Computing modernization program.
NR 40
TC 8
Z9 8
U1 2
U2 22
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
EI 1533-3876
J9 J PROPUL POWER
JI J. Propul. Power
PD MAY-JUN
PY 2014
VL 30
IS 3
BP 558
EP 575
DI 10.2514/1.B34929
PG 18
WC Engineering, Aerospace
SC Engineering
GA AH7ZI
UT WOS:000336353500005
ER
PT J
AU Mao, HS
Wirz, RE
Goebel, DM
AF Mao, Hann-Shin
Wirz, Richard E.
Goebel, Dan M.
TI Plasma Structure of Miniature Ring-Cusp Ion Thruster Discharges
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
ID PERFORMANCE
AB Previous miniature ion thruster studies have demonstrated impressive performance using ring-cusp discharges. These studies suggest that the magnetic field must be sufficiently strong to increase primary electron confinement times for ionization, but weak enough to allow plasma electrons to escape and maintain the plasma potential necessary for ionization. To investigate these phenomena, an experiment was developed to allow detailed measurements of the internal structure and characteristics of a miniature ring-cusp discharge. These measurements provide spatially resolved values for plasma density, electron temperature, and plasma potential along a meridian plane. The magnetic field configuration is arranged as a quasi-periodic domain in order to generalize the findings to all multipole discharges. The results show that the magnetic field strength drives the plasma structure, and the dependence on discharge power can be removed with proper scaling of the plasma parameters. The stronger magnetic field results in a higher peak plasma density, but relatively low discharge utilization efficiency. In addition, the potential measurements indicate the likely onset of discharge instability. In contrast, the weaker magnetic field, or baseline. configuration, better uses the volume of the chamber. This leads to a higher and more uniform density near the downstream end of the discharge where ion extraction would occur, implying superior discharge utilization.
C1 [Mao, Hann-Shin; Wirz, Richard E.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Goebel, Dan M.] CALTECH, Jet Prop Lab, Prop & Mat Engn Sect, Pasadena, CA 91109 USA.
RP Mao, HS (reprint author), Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
NR 20
TC 0
Z9 0
U1 5
U2 13
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
EI 1533-3876
J9 J PROPUL POWER
JI J. Propul. Power
PD MAY-JUN
PY 2014
VL 30
IS 3
BP 628
EP 636
DI 10.2514/1.B34759
PG 9
WC Engineering, Aerospace
SC Engineering
GA AH7ZI
UT WOS:000336353500010
ER
PT J
AU Talukder, A
Panangadan, A
AF Talukder, Ashit
Panangadan, Anand
TI Extreme event detection and assimilation from multimedia sources
SO MULTIMEDIA TOOLS AND APPLICATIONS
LA English
DT Article
DE Event detection; Information retrieval; Matching; Multimedia;
Representation; Search; Spatio-temporal trajectory; Tracking
ID VIDEO; MODEL
AB A new event-based multimedia processing framework for detection, retrieval, and cross-media content assimilation of geo-spatiotemporal phenomena is described. Multimedia information relevant to geo-spatiotemporal events are available from sources such as remote satellites, in-situ sensors as image streams, and other outlets such as news articles, weather bulletins as text documents and in various formats, each with widely varying properties. We pose an event-based framework to automatically detect geo-spatiotemporal phenomena from raw untagged remote-sensing satellite image streams, extract attributes for such events, match the spatiotemporal properties of the detected phenomenon with events in a database to automatically derive a media-independent event description, and subsequently use the media-independent event descriptions to assimilate relevant information of the same event across other media sources from the web using a mashup. A virtual globe interface enables simultaneous visualization of the assimilated spatiotemporal information annotated with Internet sources. This framework is demonstrated for the automatic detection of tropical cyclones from satellite imagery followed by the retrieval and assimilation of related information from government-run weather sites and commercial news portals.
C1 [Talukder, Ashit] NIST, Gaithersburg, MD 20899 USA.
[Panangadan, Anand] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Talukder, A (reprint author), NIST, 100 Bur Dr,Mail Stop 8940, Gaithersburg, MD 20899 USA.
EM ashit.talukder@nist.gov; Anand.V.Panangadan@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA) Applied Information
Systems Research (AISR) Program
FX The research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology with funding
from the National Aeronautics and Space Administration (NASA) Applied
Information Systems Research (AISR) Program. The authors acknowledge the
contributions of Eric Rigor, Andrew Bingham, and Shen-shyang Ho.
NR 38
TC 1
Z9 1
U1 0
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1380-7501
EI 1573-7721
J9 MULTIMED TOOLS APPL
JI Multimed. Tools Appl.
PD MAY
PY 2014
VL 70
IS 1
BP 237
EP 261
DI 10.1007/s11042-012-1088-y
PG 25
WC Computer Science, Information Systems; Computer Science, Software
Engineering; Computer Science, Theory & Methods; Engineering, Electrical
& Electronic
SC Computer Science; Engineering
GA AI4AK
UT WOS:000336807300010
ER
PT J
AU Freeman, JC
AF Freeman, Jon C.
TI Self-heating in semiconductors: A comparative study
SO SOLID-STATE ELECTRONICS
LA English
DT Article
DE Heat generation; Bipolar semiconductor; Numerical simulation;
Thermoelectric
ID DEVICES; GENERATION; CONDUCTION; SIMULATION; DIODES; MODEL; SI
AB A new expression for the source term H, in the heat flow equation is developed for bipolar semiconductors. This term consists of heat generated by carrier-lattice collisions, recombination of electrons and holes, and other processes. The expression allows self-consistent calculations of self-heating in any device. The derivation is based on thermoelectric concepts. There exists several expressions for H in the general literature for calculating the temperature field, and the presently developed one is compared with the older ones. Discrepancies exist between all of the formulas and reasons for them are given. (C) 2014 Published by Elsevier Ltd.
C1 Natl Aeronaut & Space Adm, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Freeman, JC (reprint author), Natl Aeronaut & Space Adm, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM freem231@umn.edu
NR 43
TC 1
Z9 1
U1 3
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0038-1101
EI 1879-2405
J9 SOLID STATE ELECTRON
JI Solid-State Electron.
PD MAY
PY 2014
VL 95
BP 8
EP 14
DI 10.1016/j.sse.2014.02.005
PG 7
WC Engineering, Electrical & Electronic; Physics, Applied; Physics,
Condensed Matter
SC Engineering; Physics
GA AI3QI
UT WOS:000336776600002
ER
PT J
AU Yamamoto, N
Gdoutos, E
Toda, R
White, V
Manohara, H
Daraio, C
AF Yamamoto, Namiko
Gdoutos, Eleftherios
Toda, Risaku
White, Victor
Manohara, Harish
Daraio, Chiara
TI Thin Films with Ultra-low Thermal Expansion
SO ADVANCED MATERIALS
LA English
DT Article
DE ultra-low thermal expansion; thermal stability; thin films; metals;
microstructures
ID DIGITAL-IMAGE-CORRELATION; HIGH STIFFNESS; OPTIMIZATION; COEFFICIENT;
SYSTEMS; DESIGN
C1 [Yamamoto, Namiko; Gdoutos, Eleftherios; Daraio, Chiara] CALTECH, Grad Aerosp Labs, Pasadena, CA 91125 USA.
[Toda, Risaku; White, Victor; Manohara, Harish] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Daraio, Chiara] Swiss Fed Inst Technol, Dept Mech & Proc Engn, CH-8092 Zurich, Switzerland.
RP Yamamoto, N (reprint author), CALTECH, Grad Aerosp Labs, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM namikoy@caltech.edu
RI Daraio, Chiara/N-2170-2015
OI Daraio, Chiara/0000-0001-5296-4440
FU Keck Institute for Space Studies, Center Innovation Funds (CIF) from Jet
Propulsion Laboratory; Government sponsorship
FX The authors acknowledge Prof. Craig A. Steeves from University of
Toronto, Mr. Keith Patterson from California Institute of Technology,
Dr. Andrew A. Shapiro and Dr. James Breckinridge from Jet Propulsion
Laboratory, and Ms. Elisha Byrne from the Correlated Solutions, Inc. for
helpful discussions and technical assistance. This work was supported by
the Keck Institute for Space Studies, Center Innovation Funds (CIF) from
Jet Propulsion Laboratory. A 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. (c)
2010 California Institute of Technology. Government sponsorship
acknowledged.
NR 23
TC 11
Z9 11
U1 3
U2 25
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 0935-9648
EI 1521-4095
J9 ADV MATER
JI Adv. Mater.
PD MAY
PY 2014
VL 26
IS 19
BP 3076
EP 3080
DI 10.1002/adma.201304997
PG 5
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied;
Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA AH1GW
UT WOS:000335869100017
PM 24677188
ER
PT J
AU Han, JW
Oh, JS
Meyyappan, M
AF Han, Jin-Woo
Oh, Jae Sub
Meyyappan, M.
TI Cofabrication of Vacuum Field Emission Transistor (VFET) and MOSFET
SO IEEE TRANSACTIONS ON NANOTECHNOLOGY
LA English
DT Article
DE Beyond CMOS; field emission; insulated-gate; monolithic integration;
more than Moore; vacuum field emission transistor (VFET)
ID TRIODE; FABRICATION; AMPLIFIER
AB Co-fabrication of a nanoscale vacuum field emission transistor (VFET) and a metal-oxide-semiconductor field effect transistor (MOSFET) is demonstrated on a silicon-on-insulator wafer. The insulated-gate VFET with a gap distance of 100 nm is achieved by using a conventional 0.18-mu m process technology and subsequent photoresist ashing process. The VFET shows a turn-on voltage of 2 V at a cell current of 2 nA and a cell current of 3 mu A at the operation voltage of 10 V with an ON/OFF current ratio of 10(4). The gap distance between the cathode and anode in the VFET is defined to be less than the mean free path of electrons in air, and consequently, the operation voltage is reduced to be less than the ionization potential of air molecules. This allows the relaxation of the vacuum requirement. The present integration scheme can be useful as it combines the advantages of both structures on the same chip.
C1 [Han, Jin-Woo; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Oh, Jae Sub] Natl Nanofab Ctr, Taejon 305701, South Korea.
RP Han, JW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
EM jin-woo.han@nasa.gov; jsoh@nnfc.re.kr; m.meyyappan@nasa.gov
FU Center Innovation Fund at NASA Ames Research Center
FX This work was supported by the Center Innovation Fund at NASA Ames
Research Center. The review of this paper was arranged by Associate
Editor M. M. De Souza.
NR 13
TC 8
Z9 8
U1 3
U2 26
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1536-125X
EI 1941-0085
J9 IEEE T NANOTECHNOL
JI IEEE Trans. Nanotechnol.
PD MAY
PY 2014
VL 13
IS 3
BP 464
EP 468
DI 10.1109/TNANO.2014.2310774
PG 5
WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology;
Materials Science, Multidisciplinary; Physics, Applied
SC Engineering; Science & Technology - Other Topics; Materials Science;
Physics
GA AH4IQ
UT WOS:000336091000011
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.
[Siegel, Peter H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA.
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 MAY
PY 2014
VL 4
IS 3
BP 293
EP 293
DI 10.1109/TTHZ.2014.2315757
PG 1
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA AH6EH
UT WOS:000336223000001
ER
PT J
AU Zhang, XY
Tan, B
Yu, YY
AF Zhang, Xiaoyang
Tan, Bin
Yu, Yunyue
TI Interannual variations and trends in global land surface phenology
derived from enhanced vegetation index during 1982-2010
SO INTERNATIONAL JOURNAL OF BIOMETEOROLOGY
LA English
DT Article
DE Long-term global phenology; Interannual variation; Trend; Remote sensing
ID CONTERMINOUS UNITED-STATES; HIGH-RESOLUTION RADIOMETER; NET PRIMARY
PRODUCTION; TIME-SERIES; CANOPY PHENOLOGY; GROWING-SEASON; SATELLITE
DATA; TEMPORAL VARIATION; AVHRR DATA; DATA SET
AB Land surface phenology is widely retrieved from satellite observations at regional and global scales, and its long-term record has been demonstrated to be a valuable tool for reconstructing past climate variations, monitoring the dynamics of terrestrial ecosystems in response to climate impacts, and predicting biological responses to future climate scenarios. This study detected global land surface phenology from the advanced very high resolution radiometer (AVHRR) and the Moderate Resolution Imaging Spectroradiometer (MODIS) data from 1982 to 2010. Based on daily enhanced vegetation index at a spatial resolution of 0.05 degrees, we simulated the seasonal vegetative trajectory for each individual pixel using piecewise logistic models, which was then used to detect the onset of greenness increase (OGI) and the length of vegetation growing season (GSL). Further, both overall interannual variations and pixel-based trends were examined across Koeppen's climate regions for the periods of 1982-1999 and 2000-2010, respectively. The results show that OGI and GSL varied considerably during 1982-2010 across the globe. Generally, the interannual variation could be more than a month in precipitation-controlled tropical and dry climates while it was mainly less than 15 days in temperature-controlled temperate, cold, and polar climates. OGI, overall, shifted early, and GSL was prolonged from 1982 to 2010 in most climate regions in North America and Asia while the consistently significant trends only occurred in cold climate and polar climate in North America. The overall trends in Europe were generally insignificant. Over South America, late OGI was consistent (particularly from 1982 to 1999) while either positive or negative GSL trends in a climate region were mostly reversed between the periods of 1982-1999 and 2000-2010. In the Northern Hemisphere of Africa, OGI trends were mostly insignificant, but prolonged GSL was evident over individual climate regions during the last 3 decades. OGI mainly showed late trends in the Southern Hemisphere of Africa while GSL was reversed from reduced GSL trends (1982-1999) to prolonged trends (2000-2010). In Australia, GSL exhibited considerable interannual variation, but the consistent trend lacked presence in most regions. Finally, the proportion of pixels with significant trends was less than 1 % in most of climate regions although it could be as large as 10 %.
C1 [Zhang, Xiaoyang] S Dakota State Univ, GSCE, Brookings, SD 57007 USA.
[Tan, Bin] NASA Goddard Space Flight Ctr, Earth Resources Technol Inc, Greenbelt, MD 20771 USA.
[Yu, Yunyue] NOAA NESDIS STAR, College Pk, MD 20740 USA.
RP Zhang, XY (reprint author), S Dakota State Univ, GSCE, 1021 Medary Ave,Wecota Hall 506B, Brookings, SD 57007 USA.
EM xiaoyang.zhang@sdstate.edu
RI Yu, Yunyue/F-5636-2010
FU NASA MEaSUREs [NNX08AT05A]
FX This work was partially supported by NASA MEaSUREs contract NNX08AT05A.
We wish to thank Kamel Didan and Armando Barreto Munoz at the University
of Arizona for providing long-term EVI2 detest.
NR 67
TC 21
Z9 21
U1 4
U2 53
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0020-7128
EI 1432-1254
J9 INT J BIOMETEOROL
JI Int. J. Biometeorol.
PD MAY
PY 2014
VL 58
IS 4
BP 547
EP 564
DI 10.1007/s00484-014-0802-z
PG 18
WC Biophysics; Environmental Sciences; Meteorology & Atmospheric Sciences;
Physiology
SC Biophysics; Environmental Sciences & Ecology; Meteorology & Atmospheric
Sciences; Physiology
GA AH7QU
UT WOS:000336329300013
PM 24639008
ER
PT J
AU Dubey, A
Antypas, K
Calder, AC
Daley, C
Fryxell, B
Gallagher, JB
Lamb, DQ
Lee, D
Olson, K
Reid, LB
Rich, P
Ricker, PM
Riley, KM
Rosner, R
Siegel, A
Taylor, NT
Weide, K
Timmes, FX
Vladimirova, N
ZuHone, J
AF Dubey, Anshu
Antypas, Katie
Calder, Alan C.
Daley, Chris
Fryxell, Bruce
Gallagher, J. Brad
Lamb, Donald Q.
Lee, Dongwook
Olson, Kevin
Reid, Lynn B.
Rich, Paul
Ricker, Paul M.
Riley, Katherine M.
Rosner, Robert
Siegel, Andrew
Taylor, Noel T.
Weide, Klaus
Timmes, Francis X.
Vladimirova, Natasha
ZuHone, John
TI Evolution of FLASH, a multi-physics scientific simulation code for
high-performance computing
SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS
LA English
DT Article
DE FLASH; scientific application code; multi-physics; multi-scale;
community code; software evolution
ID STAGGERED MESH SCHEME; RAYLEIGH-TAYLOR; MAGNETOHYDRODYNAMICS;
HYDRODYNAMICS; ASTROPHYSICS; DIMENSIONS; PLUTO; FLOWS
AB The FLASH code has evolved into a modular and extensible scientific simulation software system over the decade of its existence. During this time it has been cumulatively used by over a thousand researchers to investigate problems in astrophysics, cosmology, and in some areas of basic physics, such as turbulence. Recently, many new capabilities have been added to the code to enable it to simulate problems in high-energy density physics. Enhancements to these capabilities continue, along with enhancements enabling simulations of problems in fluid-structure interactions. The code started its life as an amalgamation of already existing software packages and sections of codes developed independently by various participating members of the team for other purposes. The code has evolved through a mixture of incremental and deep infrastructural changes. In the process, it has undergone four major revisions, three of which involved a significant architectural advancement. Along the way, a software process evolved that addresses the issues of code verification, maintainability, and support for the expanding user base. The software process also resolves the conflicts arising out of being in development and production simultaneously with multiple research projects, and between performance and portability. This paper describes the process of code evolution with emphasis on the design decisions and software management policies that have been instrumental in the success of the code. The paper also makes the case for a symbiotic relationship between scientific research and good software engineering of the simulation software.
C1 [Dubey, Anshu; Daley, Chris; Gallagher, J. Brad; Lamb, Donald Q.; Lee, Dongwook; Taylor, Noel T.; Weide, Klaus] Univ Chicago, Flash Ctr Computat Sci, Chicago, IL 60637 USA.
[Dubey, Anshu] Lawrence Berkeley Natl Lab, Computat Res Div, Berkeley, CA USA.
[Antypas, Katie; Daley, Chris] Lawrence Berkeley Natl Lab, Natl Energy Res Sci Comp Ctr, Berkeley, CA USA.
[Calder, Alan C.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY USA.
[Calder, Alan C.] SUNY Stony Brook, Inst Adv Computat Sci, Stony Brook, NY USA.
[Gallagher, J. Brad; Lamb, Donald Q.; Lee, Dongwook; Rosner, Robert; Weide, Klaus] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Lamb, Donald Q.; Lee, Dongwook; Rosner, Robert; Siegel, Andrew] Argonne Natl Lab, Math & Comp Sci Div, Argonne, IL 60439 USA.
[Fryxell, Bruce] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Lamb, Donald Q.; Lee, Dongwook; Rosner, Robert] Univ Chicago, Computat Inst, Chicago, IL 60637 USA.
[Lamb, Donald Q.; Lee, Dongwook; Rosner, Robert] Argonne Natl Lab, Argonne, IL 60439 USA.
[Olson, Kevin] Drexel Univ, Dept Phys, Philadelphia, PA USA.
[Reid, Lynn B.] Univ Western Australia, Nedlands, WA 6009, Australia.
[Reid, Lynn B.] CDM Smith, Brisbane, Qld, Australia.
[Rich, Paul; Riley, Katherine M.] Argonne Natl Lab, Argonne Leadership Comp Facil, Argonne, IL 60439 USA.
[Ricker, Paul M.] Univ Illinois, Dept Astron, Chicago, IL 60680 USA.
[Timmes, Francis X.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Timmes, Francis X.] Univ Notre Dame, Joint Inst Nucl Astrophys, Notre Dame, IN 46556 USA.
[Vladimirova, Natasha] Univ New Mexico, Dept Math & Stat, Albuquerque, NM 87131 USA.
[ZuHone, John] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD USA.
RP Dubey, A (reprint author), Univ Chicago, 5747 S Ellis Ave, Chicago, IL 60637 USA.
EM adubey@lbl.gov
OI Weide, Klaus/0000-0001-9869-9750
FU DOE [B523820]; US DOE NNSA ASC through the Argonne Institute for
Computing in Science [57789]; NSF [5-27429]
FX The FLASH code was in part developed by the DOE-supported ASC/Alliance
Center for Astrophysical Thermonuclear Flashes at the University of
Chicago (grant number B523820). The continued development has been
supported in part by the US DOE NNSA ASC through the Argonne Institute
for Computing in Science (field work proposal 57789) and by a NSF
Peta-apps grant (grant number 5-27429).
NR 33
TC 2
Z9 2
U1 0
U2 8
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1094-3420
EI 1741-2846
J9 INT J HIGH PERFORM C
JI Int. J. High Perform. Comput. Appl.
PD MAY
PY 2014
VL 28
IS 2
SI SI
BP 225
EP 237
DI 10.1177/1094342013505656
PG 13
WC Computer Science, Hardware & Architecture; Computer Science,
Interdisciplinary Applications; Computer Science, Theory & Methods
SC Computer Science
GA AH6EE
UT WOS:000336222700006
ER
PT J
AU Williams, CR
Bringi, VN
Carey, LD
Chandrasekar, V
Gatlin, PN
Haddad, ZS
Meneghini, R
Munchak, SJ
Nesbitt, SW
Petersen, WA
Tanelli, S
Tokay, A
Wilson, A
Wolff, DB
AF Williams, Christopher R.
Bringi, V. N.
Carey, Lawrence D.
Chandrasekar, V.
Gatlin, Patrick N.
Haddad, Ziad S.
Meneghini, Robert
Munchak, S. Joseph
Nesbitt, Stephen W.
Petersen, Walter A.
Tanelli, Simone
Tokay, Ali
Wilson, Anna
Wolff, David B.
TI Describing the Shape of Raindrop Size Distributions Using Uncorrelated
Raindrop Mass Spectrum Parameters
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
DE Precipitation; Rainfall; Algorithms; Radars; Radar observations;
Satellite observations
ID FREQUENCY RADAR MEASUREMENTS; TRMM PRECIPITATION RADAR;
GAMMA-DISTRIBUTIONS; RETRIEVAL ALGORITHM; PROFILING ALGORITHM; MOMENT
ESTIMATORS; VIDEO DISDROMETER; MICROPHYSICS; ERRORS; BIAS
AB Rainfall retrieval algorithms often assume a gamma-shaped raindrop size distribution (DSD) with three mathematical parameters N-w, D-m, and . If only two independent measurements are available, as with the dual-frequency precipitation radar on the Global Precipitation Measurement (GPM) mission core satellite, then retrieval algorithms are underconstrained and require assumptions about DSD parameters. To reduce the number of free parameters, algorithms can assume that is either a constant or a function of D-m. Previous studies have suggested - constraints [where = (4 + )/D-m], but controversies exist over whether - constraints result from physical processes or mathematical artifacts due to high correlations between gamma DSD parameters. This study avoids mathematical artifacts by developing joint probability distribution functions (joint PDFs) of statistically independent DSD attributes derived from the raindrop mass spectrum. These joint PDFs are then mapped into gamma-shaped DSD parameter joint PDFs that can be used in probabilistic rainfall retrieval algorithms as proposed for the GPM satellite program. Surface disdrometer data show a high correlation coefficient between the mass spectrum mean diameter D-m and mass spectrum standard deviation sigma(m). To remove correlations between DSD attributes, a normalized mass spectrum standard deviation is constructed to be statistically independent of D-m, with representing the most likely value and std representing its dispersion. Joint PDFs of D-m and are created from D-m and . A simple algorithm shows that rain-rate estimates had smaller biases when assuming the DSD breadth of than when assuming a constant .
C1 [Williams, Christopher R.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Williams, Christopher R.] NOAA, ESRL Phys Sci Div, Boulder, CO USA.
[Bringi, V. N.; Chandrasekar, V.] Colorado State Univ, Ft Collins, CO 80523 USA.
[Carey, Lawrence D.] Univ Alabama, Huntsville, AL 35899 USA.
[Gatlin, Patrick N.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Haddad, Ziad S.; Tanelli, Simone] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Meneghini, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Munchak, S. Joseph] Univ Maryland, College Pk, MD 20742 USA.
[Nesbitt, Stephen W.] Univ Illinois, Urbana, IL USA.
[Petersen, Walter A.; Wolff, David B.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Tokay, Ali] Univ Maryland Baltimore Cty, Greenbelt, MD USA.
[Wilson, Anna] Duke Univ, Durham, NC USA.
RP Williams, CR (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, 216 UCB, Boulder, CO 80309 USA.
EM christopher.williams@colorado.edu
RI Williams, Christopher/A-2723-2015; Measurement, Global/C-4698-2015;
OI Williams, Christopher/0000-0001-9394-8850; Gatlin,
Patrick/0000-0001-9345-1457
FU NASA Global Precipitation Measurement (GPM) mission [NNX13AI94G,
NNX10AM54G, NNX13AF89G, NNX12AD03A, NNX10AP84G, NNX13AF86G, NNX13AJ55G,
NNX13AI89G, NNX10AH66G]; NASA Precipitation Measurement Missions (PMM)
FX Support for this work was provided by Ramesh Kakar under the NASA
Precipitation Measurement Missions (PMM) and NASA Global Precipitation
Measurement (GPM) mission, including Grants NNX13AI94G, NNX10AM54G,
NNX13AF89G, NNX12AD03A, NNX10AP84G, NNX13AF86G, NNX13AJ55G, NNX13AI89G,
and NNX10AH66G. The authors thank Dr. Merhala Thurai for her insightful
discussions.
NR 37
TC 17
Z9 17
U1 5
U2 20
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD MAY
PY 2014
VL 53
IS 5
BP 1282
EP 1296
DI 10.1175/JAMC-D-13-076.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AG6ZF
UT WOS:000335567000010
ER
PT J
AU Dong, XQ
Xi, BK
Kennedy, A
Minnis, P
Wood, R
AF Dong, Xiquan
Xi, Baike
Kennedy, Aaron
Minnis, Patrick
Wood, Robert
TI A 19-Month Record of Marine Aerosol- Cloud-Radiation Properties Derived
from DOE ARM Mobile Facility Deployment at the Azores. Part I: Cloud
Fraction and Single-Layered MBL Cloud Properties
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Boundary layer; Cloud cover; Diurnal effects; Subsidence; Aerosols;
Cloud microphysics
ID GROUND-BASED MEASUREMENTS; LIQUID WATER PATH; GENERAL-CIRCULATION
MODELS; WARM STRATOCUMULUS CLOUDS; BOUNDARY-LAYER; STRATIFORM CLOUDS;
MICROPHYSICAL CONTRASTS; STRATUS; CLIMATE; ASTEX
AB A 19-month record of total and single-layered low (<3 km), middle (3-6 km), and high (>6 km) cloud fractions (CFs) and the single-layered marine boundary layer (MBL) cloud macrophysical and microphysical properties was generated from ground-based measurements at the Atmospheric Radiation Measurement Program (ARM) Azores site between June 2009 and December 2010. This is the most comprehensive dataset of marine cloud fraction and MBL cloud properties. The annual means of total CF and single-layered low, middle, and high CFs derived from ARM radar and lidar observations are 0.702, 0.271, 0.01, and 0.106, respectively. Greater total and single-layered high (>6 km) CFs occurred during the winter, whereas single-layered low (<3 km) CFs were more prominent during summer. Diurnal cycles for both total and low CFs were stronger during summer than during winter. The CFs are bimodally distributed in the vertical with a lower peak at similar to 1 km and a higher peak between 8 and 11 km during all seasons, except summer when only the low peak occurs. Persistent high pressure and dry conditions produce more single-layered MBL clouds and fewer total clouds during summer, whereas the low pressure and moist air masses during winter generate more total and multilayered clouds, and deep frontal clouds associated with midlatitude cyclones.The seasonal variations of cloud heights and thickness are also associated with the seasonal synoptic patterns. The MBL cloud layer is low, warm, and thin with large liquid water path (LWP) and liquid water content (LWC) during summer, whereas during winter it is higher, colder, and thicker with reduced LWP and LWC. The cloud LWP and LWC values are greater at night than during daytime. The monthly mean daytime cloud droplet effective radius r(e) values are nearly constant, while the daytime droplet number concentration N-d basically follows the LWC variation. There is a strong correlation between cloud condensation nuclei (CCN) concentration N-CCN and N-d during January-May, probably due to the frequent low pressure systems because upward motion brings more surface CCN to cloud base (well-mixed boundary layer). During summer and autumn, the correlation between N-d and N-CCN is not as strong as that during January-May because downward motion from high pressure systems is predominant. Compared to the compiled aircraft in situ measurements during the Atlantic Stratocumulus Transition Experiment (ASTEX), the cloud microphysical retrievals in this study agree well with historical aircraft data. Different air mass sources over the ARM Azores site have significant impacts on the cloud microphysical properties and surface CCN as demonstrated by great variability in N-CCN and cloud microphysical properties during some months.
C1 [Dong, Xiquan; Xi, Baike; Kennedy, Aaron] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA.
[Minnis, Patrick] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA USA.
[Wood, Robert] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
RP Dong, XQ (reprint author), Univ N Dakota, Dept Atmospher Sci, 4149 Campus Rd,Box 9006, Grand Forks, ND 58202 USA.
EM dong@aero.und.edu
RI Wood, Robert/A-2989-2008; Minnis, Patrick/G-1902-2010;
OI Wood, Robert/0000-0002-1401-3828; Minnis, Patrick/0000-0002-4733-6148;
Dong, Xiquan/0000-0002-3359-6117
FU U.S. Department of Energy (DOE) Office of Energy Research, Office of
Health and Environmental Research, Environmental Sciences Division; NASA
CERES project at the University of North Dakota project [NNX10AI05G];
DOE ASR project at the University of North Dakota [DE-SC0008468]; DOE
ASR project at the University of Washington [DE-SC0006865MOD0002]; DOE
ASR program under Interagency Grant [DE-SC0000991/003]
FX The data were obtained from the Atmospheric Radiation Measurement (ARM)
Program sponsored by the U.S. Department of Energy (DOE) Office of
Energy Research, Office of Health and Environmental Research,
Environmental Sciences Division. This study was primarily supported by
the NASA CERES project at the University of North Dakota project under
Grant NNX10AI05G and by the DOE ASR project at the University of North
Dakota under a grant with Award DE-SC0008468. Dr. Robert Wood was
supported by the DOE ASR project at the University of Washington with
Award DE-SC0006865MOD0002. Patrick Minnis was supported by the DOE ASR
program under Interagency Grant DE-SC0000991/003. Special thanks to Dr.
Long, who provided the clear-sky SW fluxes over the ARM Azores site.
NR 51
TC 15
Z9 15
U1 2
U2 16
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 MAY
PY 2014
VL 27
IS 10
BP 3665
EP 3682
DI 10.1175/JCLI-D-13-00553.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AG6PO
UT WOS:000335541100012
ER
PT J
AU Baker, NC
Huang, HP
AF Baker, Noel C.
Huang, Huei-Ping
TI A Comparative Study of Precipitation and Evaporation between CMIP3 and
CMIP5 Climate Model Ensembles in Semiarid Regions
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Europe; North America; Rainfall; Water budget; Ensembles; Ensembles
ID GLOBAL PRECIPITATION; VARIABILITY; REANALYSES; MONSOON; GPCP; ERA
AB The twentieth-century climatology and twenty-first-century trend in precipitation P, evaporation E, and P - E for selected semiarid U.S. Southwest and Mediterranean regions are compared between ensembles from phases 3 and 5 of the Coupled Model Intercomparison Project (CMIP3 and CMIP5). The twentieth-century simulations are validated with precipitation from observation and evaporation from reanalysis. It is found that the Special Report on Emissions Scenarios (SRES) A1B simulations in CMIP3 and the simulations with representative concentration pathways (RCPs) 4.5 and 8.5 in CMIP5 produce qualitatively similar seasonal cycles of the twenty-first-century trend in P - E for both semiarid regions. For the southwestern United States, it is characterized by a strong drying trend in spring, a weak moistening trend in summer, a weak drying trend in winter, and an overall drying trend for the annual mean. For the Mediterranean region, a drying trend is simulated for all seasons with an October maximum and July minimum. The consistency between CMIP3 and CMIP5 scenarios indicates that the simulated trend is robust; however, while the trend in P - E is negative in spring for the southwestern United States for all CMIP ensembles, CMIP3 predicts a strongly negative trend in P and minor negative trend in E whereas both CMIP5 scenarios predict a nearly zero trend in P and positive trend in E. For the twentieth-century simulations, the P, E, and P - E of the two model ensembles are statistically indistinguishable for most seasons. This stagnation of the simulated climatology from CMIP3 to CMIP5 implies that the hydroclimatic variable biases have not decreased in the newer generation of models. Notably, over the southwestern United States the CMIP3 models produce too much precipitation in the cold season. This bias remains almost unchanged in CMIP5.
C1 [Baker, Noel C.; Huang, Huei-Ping] Arizona State Univ, Sch Engn Matter Transport & Energy, Tempe, AZ USA.
RP Baker, NC (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd,Mail Stop 420, Hampton, VA 23681 USA.
EM noel.c.baker@nasa.gov
FU Office of Science (BER), U.S. Department of Energy
FX This study is supported by the Office of Science (BER), U.S. Department
of Energy. The NCEP R2 data were obtained from the NOAA ESRL/PSDdata
portal (http://www.esrl.noaa.gov/psd). ECMWF ERA-Interim data have been
obtained from the ECMWF data server (http://apps.ecmwf.int/datasets/).
NR 25
TC 12
Z9 12
U1 2
U2 25
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 MAY
PY 2014
VL 27
IS 10
BP 3731
EP 3749
DI 10.1175/JCLI-D-13-00398.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AG6PO
UT WOS:000335541100016
ER
PT J
AU Holland, PR
Bruneau, N
Enright, C
Losch, M
Kurtz, NT
Kwok, R
AF Holland, Paul R.
Bruneau, Nicolas
Enright, Clare
Losch, Martin
Kurtz, Nathan T.
Kwok, Ron
TI Modeled Trends in Antarctic Sea Ice Thickness
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Antarctica; Sea ice; Southern Ocean; Climate variability; Interannual
variability; Trends
ID OCEAN MODEL; DATA ASSIMILATION; SOUTHERN-OCEAN; CMIP5 MODELS;
MASS-BALANCE; WEDDELL SEA; SNOW DEPTH; MAUD RISE; VARIABILITY;
SIMULATIONS
AB Unlike the rapid sea ice losses reported in the Arctic, satellite observations show an overall increase in Antarctic sea ice concentration over recent decades. However, observations of decadal trends in Antarctic ice thickness, and hence ice volume, do not currently exist. In this study a model of the Southern Ocean and its sea ice, forced by atmospheric reanalyses, is used to assess 1992-2010 trends in ice thickness and volume. The model successfully reproduces observations of mean ice concentration, thickness, and drift, and decadal trends in ice concentration and drift, imparting some confidence in the hindcasted trends in ice thickness. The model suggests that overall Antarctic sea ice volume has increased by approximately 30 km(3) yr(-1) (0.4% yr(-1)) as an equal result of areal expansion (20 x 10(3) km(2) yr(-1) or 0.2% yr(-1)) and thickening (1.5 mm yr(-1) or 0.2% yr(-1)). This ice volume increase is an order of magnitude smaller than the Arctic decrease, and about half the size of the increased freshwater supply from the Antarctic Ice Sheet. Similarly to the observed ice concentration trends, the small overall increase in modeled ice volume is actually the residual of much larger opposing regional trends. Thickness changes near the ice edge follow observed concentration changes, with increasing concentration corresponding to increased thickness. Ice thickness increases are also found in the inner pack in the Amundsen and Weddell Seas, where the model suggests that observed ice-drift trends directed toward the coast have caused dynamical thickening in autumn and winter. Modeled changes are predominantly dynamic in origin in the Pacific sector and thermodynamic elsewhere.
C1 [Holland, Paul R.; Bruneau, Nicolas] British Antarctic Survey, Cambridge CB3 0ET, England.
[Enright, Clare] Univ E Anglia, Tyndall Ctr Climate Change Res, Norwich NR4 7TJ, Norfolk, England.
[Losch, Martin] Alfred Wegener Inst Polar & Marine Res, Bremerhaven, Germany.
[Kurtz, Nathan T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kwok, Ron] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Holland, PR (reprint author), British Antarctic Survey, Madingley Rd, Cambridge CB3 0ET, England.
EM p.holland@bas.ac.uk
RI Holland, Paul/G-2796-2012; Kwok, Ron/A-9762-2008; Losch,
Martin/S-5896-2016;
OI Kwok, Ron/0000-0003-4051-5896; Losch, Martin/0000-0002-3824-5244;
Bruneau, Nicolas/0000-0002-9017-1000
NR 78
TC 22
Z9 22
U1 2
U2 36
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 MAY
PY 2014
VL 27
IS 10
BP 3784
EP 3801
DI 10.1175/JCLI-D-13-00301.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AG6PO
UT WOS:000335541100019
ER
PT J
AU Eingorn, M
Zhuk, A
AF Eingorn, Maxim
Zhuk, Alexander
TI Remarks on mechanical approach to observable Universe
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE cosmological perturbation theory; gravity; dark energy theory; cosmic
flows
ID DARK ENERGY
AB We consider the Universe deep inside the cell of uniformity. At these scales, the Universe is filled with inhomogeneously distributed discrete structures (galaxies, groups and clusters of galaxies), which perturb the background Friedmann model. Here, the mechanical approach (Eingorn & Zhuk, 2012) is the most appropriate to describe the dynamics of the inhomogeneities which is defined, on the one hand, by gravitational potentials of inhomogeneities and, on the other hand, by the cosmological expansion of the Universe. In this paper, we present additional arguments in favor of this approach. First, we estimate the size of the cell of uniformity. With the help of the standard methods of statistical physics and for the galaxies of the type of the Milky Way and Andromeda, we get that it is of the order of 190 Mpc which is rather close to observations. Then, we show that the nonrelativistic approximation (with respect to the peculiar velocities) is valid for z less than or similar to 10, i.e. approximately for 13 billion years from the present moment. We consider scalar perturbations and, within the ACDM model, justify the main equations. Moreover, we demonstrate that radiation can be naturally incorporated into our scheme. This emphasizes the viability of our approach. This approach gives a possibility to analyze different cosmological models and compare them with the observable Universe. For example, we indicate some problematic aspects of the spatially flat models. Such models require a rather specific distribution of the inhomogeneities to get a finite potential at any points outside gravitating masses. We also criticize the application of the Schwarzschild-de Sitter solution to the description of the motion of test bodies on the cosmological background.
C1 [Eingorn, Maxim] N Carolina Cent Univ, CREST, Durham, NC 27707 USA.
[Eingorn, Maxim] N Carolina Cent Univ, NASA, Res Ctr, Durham, NC 27707 USA.
[Zhuk, Alexander] Odessa Natl Univ, Astron Observ, UA-65082 Odessa, Ukraine.
RP Eingorn, M (reprint author), N Carolina Cent Univ, CREST, Fayetteville St 1801, Durham, NC 27707 USA.
EM maxim.eingorn@gmail.com; ai.zhuk2@gmail.com
RI Eingorn, Maxim/L-1543-2014
OI Eingorn, Maxim/0000-0002-1545-7818
FU NSF CREST award [HRD-1345219]; NASA grant [NNX09AV07A]
FX The work of M. Eingorn was supported by NSF CREST award HRD-1345219 and
NASA grant NNX09AV07A.
NR 21
TC 17
Z9 17
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD MAY
PY 2014
IS 5
AR 024
DI 10.1088/1475-7516/2014/05/024
PG 19
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AH4JC
UT WOS:000336092200026
ER
PT J
AU DeGuzman, V
Vercoutere, W
Shenasa, H
Deamer, D
AF DeGuzman, Veronica
Vercoutere, Wenonah
Shenasa, Hossein
Deamer, David
TI Generation of Oligonucleotides Under Hydrothermal Conditions by
Non-enzymatic Polymerization
SO JOURNAL OF MOLECULAR EVOLUTION
LA English
DT Article
DE RNA; Condensation reactions; Hydrolysis; Organizing matrix; Prebiotic
chemistry
ID POLYNUCLEOTIDE MOLECULES; RNA MOLECULES; ORIGIN; LIFE; DISCRIMINATION;
EVOLUTION; ACID; RIBOZYME; CHANNEL; VENTS
AB We previously reported that 5'-mononucleotides organized within a multilamellar lipid matrix can produce oligomers in the anhydrous phase of hydration-dehydration (HD) cycles. However, hydrolysis of oligomers can occur during hydration, and it is important to better understand the steady state in which ester bond synthesis is balanced by hydrolysis. In order to study condensation products of mononucleotides and hydrolysis of their polymers, we established a simulation of HD cycles that would occur on the early Earth when volcanic land masses emerged from the ocean over 4 billion years ago. At this stage on early Earth, precipitation produced hydrothermal fields characterized by small aqueous pools undergoing evaporation and refilling at elevated temperatures. Here, we confirm that under these conditions, the chemical potential made available by cycles of hydration and dehydration is sufficient to drive synthesis of ester bonds. If 5'-mononucleotides are in solution at millimolar concentrations, then oligomers resembling RNA are synthesized and exist in a steady state with their monomers. Furthermore, if the mononucleotides can form complementary base pairs, then some of the products have properties suggesting that secondary structures are present, including duplex species stabilized by hydrogen bonds.
C1 [DeGuzman, Veronica; Vercoutere, Wenonah] NASA, Ames Res Ctr, Adv Studies Lab, Moffett Field, CA 94035 USA.
[Shenasa, Hossein; Deamer, David] Univ Calif Santa Cruz, Dept Biomol Engn, Santa Cruz, CA 95064 USA.
RP Deamer, D (reprint author), Univ Calif Santa Cruz, Dept Biomol Engn, Santa Cruz, CA 95064 USA.
EM deamer@soe.ucsc.edu
FU Lonsdale Research Award
FX This investigation was supported by a Lonsdale Research Award, funded by
a generous gift from Harry Lonsdale.
NR 31
TC 10
Z9 18
U1 1
U2 38
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2844
EI 1432-1432
J9 J MOL EVOL
JI J. Mol. Evol.
PD MAY
PY 2014
VL 78
IS 5
BP 251
EP 262
DI 10.1007/s00239-014-9623-2
PG 12
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA AI1IE
UT WOS:000336603400003
PM 24821106
ER
PT J
AU Law, J
Van Baalen, M
Foy, M
Mason, SS
Mendez, C
Wear, ML
Meyers, VE
Alexander, D
AF Law, Jennifer
Van Baalen, Mary
Foy, Millennia
Mason, Sara S.
Mendez, Claudia
Wear, Mary L.
Meyers, Valerie E.
Alexander, David
TI Relationship Between Carbon Dioxide Levels and Reported Headaches on the
International Space Station
SO JOURNAL OF OCCUPATIONAL AND ENVIRONMENTAL MEDICINE
LA English
DT Article
ID CEREBRAL-BLOOD-FLOW; AIR SUPPLY RATE; CO2 CONCENTRATIONS; PERFORMANCE;
VENTILATION; RESPONSES; SYMPTOMS
AB Objective: Because of anecdotal reports of CO2-related symptoms onboard the International Space Station (ISS), the relationship between CO2 and in-flight headaches was analyzed.
Methods: Headache reports and CO2 measurements were obtained, and arithmetic means and single-point maxima were determined for 24-hour and 7-day periods. Multiple imputation addressed missing data, and logistic regression modeled the relationship between CO2, headache probability, and covariates.
Results: CO2 level, age at launch, time in-flight, and data source were significantly associated with headache. For each 1-mm Hg increase in CO2, the odds of a crew member reporting a headache doubled. To keep the risk of headache below 1%, average 7-day CO2 would need to be maintained below 2.5 mm Hg (current ISS range: 1 to 9 mm Hg).
Conclusions: Although headache incidence was not high, results suggest an increased susceptibility to physiological effects of CO2 in-flight.
C1 [Law, Jennifer; Van Baalen, Mary; Meyers, Valerie E.; Alexander, David] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Foy, Millennia; Wear, Mary L.] Wyle Sci Technol & Engn, Houston, TX USA.
[Mason, Sara S.; Mendez, Claudia] MEI Technol, Houston, TX USA.
RP Law, J (reprint author), 2101 NASA Pkwy,Mail Code SD2, Houston, TX 77058 USA.
EM jennifer.t.law@nasa.gov
NR 27
TC 7
Z9 7
U1 5
U2 11
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA
SN 1076-2752
EI 1536-5948
J9 J OCCUP ENVIRON MED
JI J. Occup. Environ. Med.
PD MAY
PY 2014
VL 56
IS 5
BP 477
EP 483
DI 10.1097/JOM.0000000000000158
PG 7
WC Public, Environmental & Occupational Health
SC Public, Environmental & Occupational Health
GA AH1FZ
UT WOS:000335866500005
PM 24806559
ER
PT J
AU Love, SG
Pettit, DR
Messenger, SR
AF Love, Stanley G.
Pettit, Donald R.
Messenger, Scott R.
TI Particle aggregation in microgravity: Informal experiments on the
International Space Station
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID PLANETESIMAL FORMATION; DUST AGGREGATION; SOLAR NEBULA; CHONDRULES;
STICKING; GROWTH; COAGULATION; MECHANISMS; COLLISIONS; DYNAMICS
AB We conducted experiments in space to investigate the aggregation of millimeter- and submillimeter-sized particles in microgravity, an important early step in planet formation. Particulate materials included salt (NaCl), sugar (sucrose), coffee, mica, ice, Bjurbole chondrules, ordinary and carbonaceous chondrite meteorite fragments, and acrylic and glass beads, all triply confined in clear plastic containers. Angular submillimeter particles rapidly and spontaneously formed clusters strong enough to survive turbulence in a protoplanetary nebula. Smaller particles generally aggregated more strongly and quickly than larger ones. We observed only a weak dependence of aggregation time on particle number density. We observed no strong dependence on composition. Round, smooth particles aggregated weakly or not at all. In a mixture of particle types, some phases aggregated more readily than others, creating selection effects that controlled the composition of the growing clumps. The physical process of aggregation appears to be electrostatic in nature.
C1 [Love, Stanley G.; Pettit, Donald R.] NASA, Lyndon B Johnson Space Ctr, Mail Code CB, Houston, TX 77058 USA.
[Messenger, Scott R.] NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, Mail Code KR,Astromat Res & Explorat Sci Director, 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
NR 41
TC 3
Z9 3
U1 0
U2 9
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 MAY
PY 2014
VL 49
IS 5
BP 732
EP 739
DI 10.1111/maps.12286
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AH9TE
UT WOS:000336484500002
ER
PT J
AU Veres, P
Farnocchia, D
Jedicke, R
Spoto, F
AF Veres, Peter
Farnocchia, Davide
Jedicke, Robert
Spoto, Federica
TI The Effect of Parallax and Cadence on Asteroid Impact Probabilities and
Warning Times
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID EARTH-APPROACHING ASTEROIDS; OBJECT PROCESSING SYSTEM; PAN-STARRS; ORBIT
DETERMINATION; CHELYABINSK; ASTROMETRY; EFFICIENCY; ORIGIN
AB We study the time evolution of the impact probability for synthetic, but realistic, impacting and close-approaching asteroids detected in a simulated all-sky survey. We use the impact probability to calculate the impact warning time (t(w)) as the time interval between when an object reaches a Palermo Scale value of -2 and when it impacts Earth. A simple argument shows that t(w) proportional to D-x, with the exponent in the range [1.0,1.5], and our derived value was x = 1.3 +/- 0.1. The low-precision astrometry from the single simulated all-sky survey could require many days or weeks to establish an imminent impact for asteroids larger than 100 m in diameter that are discovered far from Earth. Most close-approaching asteroids are quickly identified as not being impactors, but a size-dependent percentage, even for those larger than 50 m diameter, have a persistent impact probability of greater than 10(-6) on the day of closest approach. Thus, a single all-sky survey can be of tremendous value in identifying Earth-impacting and close-approaching asteroids in advance of their closest approach, but it can not solve the problem on its own: high-precision astrometry from other optical or radar systems is necessary to rapidly establish an object as an impactor or close approacher. We show that the parallax afforded by surveying the sky from two sites is only of benefit for a small fraction of the smallest objects detected within a couple days before impact: probably not enough to justify the increased operating costs of a two-site survey. Finally, the survey cadence within a fixed time span is relatively unimportant to the impact probability calculation. We tested three different reasonable cadences and found that one provided similar to 10 times higher (better) value for the impact probability on the discovery night for the smallest (10 m diameter) objects, but the consequences on the overall impact probability calculation are negligible.
C1 [Veres, Peter; Jedicke, Robert] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Farnocchia, Davide] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA.
[Spoto, Federica] Univ Pisa, Dept Math, I-56127 Pisa, Italy.
RP Veres, P (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM veres@ifa.hawaii.edu
FU NASA; NASA NEOO [NNX12AR65G]
FX We thank J. Tonry and L. Denneau of the ATLAS survey for assistance in
characterizing and designing a representative ATLAS survey. D.
Farnocchia was supported for this research 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. Peter Veres's Pan-STARRS MOPS
Postdoctoral Fellowship was sponsored by NASA NEOO grant No. NNX12AR65G.
NR 40
TC 0
Z9 0
U1 0
U2 2
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 MAY
PY 2014
VL 126
IS 939
BP 433
EP 444
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AI1VJ
UT WOS:000336643000001
ER
PT J
AU Tse, LA
Ganapathi, GB
Wirz, RE
Lavine, AS
AF Tse, Louis A.
Ganapathi, Gani B.
Wirz, Richard E.
Lavine, Adrienne S.
TI Spatial and temporal modeling of sub- and supercritical thermal energy
storage
SO SOLAR ENERGY
LA English
DT Article
DE Energy storage; Thermodynamic model; Transient behavior; Concentrating
solar power
ID PLANTS
AB This paper describes a thermodynamic model that simulates the discharge cycle of a single-tank thermal energy storage (TES) system that can operate from the two-phase (liquid-vapor) to supercritical regimes for storage fluid temperatures typical of concentrating solar power plants. State-of-the-art TES design utilizes a two-tank system with molten nitrate salts; one major problem is the high capital cost of the salts (International Renewable Energy Agency, 2012). The alternate approach explored here opens up the use of low-cost fluids by considering operation at higher pressures associated with the two-phase and supercritical regimes.
The main challenge to such a system is its high pressures and temperatures which necessitate a relatively high-cost containment vessel that represents a large fraction of the system capital cost. To mitigate this cost, the proposed design utilizes a single-tank TES system, effectively halving the required wall material. A single-tank approach also significantly reduces the complexity of the system in comparison to the two-tank systems, which require expensive pumps and external heat exchangers.
A thermodynamic model is used to evaluate system performance; in particular it predicts the volume of tank wall material needed to encapsulate the storage fluid. The transient temperature of the tank is observed to remain hottest at the storage tank exit, which is beneficial to system operation. It is also shown that there is an optimum storage fluid loading that generates a given turbine energy output while minimizing the required tank wall material.
Overall, this study explores opportunities to further improve current solar thermal technologies. The proposed single-tank system shows promise for decreasing the cost of thermal energy storage. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Tse, Louis A.; Wirz, Richard E.; Lavine, Adrienne S.] Univ Calif Los Angeles, Dept Mech & Aerosp Engn, Los Angeles, CA 90095 USA.
[Ganapathi, Gani B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Tse, LA (reprint author), Univ Calif Los Angeles, Dept Mech & Aerosp Engn, Los Angeles, CA 90095 USA.
EM ltse1@ucla.edu
FU ARPA-E [DE-AR0000140]; Southern California Gas Company [5660021607];
National Science Foundation [DGE-0707424]
FX This effort was supported by ARPA-E Award DE-AR0000140, Grant No.
5660021607 from the Southern California Gas Company, and Grant No.
DGE-0707424 from the National Science Foundation.
NR 20
TC 5
Z9 5
U1 1
U2 14
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0038-092X
J9 SOL ENERGY
JI Sol. Energy
PD MAY
PY 2014
VL 103
BP 402
EP 410
DI 10.1016/j.solener.2014.02.040
PG 9
WC Energy & Fuels
SC Energy & Fuels
GA AH7YR
UT WOS:000336351800036
ER
PT J
AU Nguyen, H
Katzfuss, M
Cressie, N
Braverman, A
AF Hai Nguyen
Katzfuss, Matthias
Cressie, Noel
Braverman, Amy
TI Spatio-Temporal Data Fusion for Very Large Remote Sensing Datasets
SO TECHNOMETRICS
LA English
DT Article
DE EM algorithm; Fixed rank smoothing; Kalman filter; Multivariate
geostatistics; Spatial random effects model
ID HIERARCHICAL-MODELS; CARBON-DIOXIDE; DATA SETS; SCIENCE
AB Developing global maps of carbon dioxide (CO2) mole fraction (in units of parts per million) near the Earth's surface can help identify locations where major amounts of CO2 are entering and exiting the atmosphere, thus providing valuable insights into the carbon cycle and mitigating the greenhouse effect of atmospheric CO2. Existing satellite remote sensing data do not provide measurements of the CO2 mole fraction near the surface. Japan's Greenhouse gases Observing SATellite (GOSAT) is sensitive to average CO2 over the entire column, and NASA's Atmospheric InfraRed Sounder (AIRS) is sensitive to CO2 in the middle troposphere. One might expect that lower-atmospheric CO2 could be inferred by differencing GOSAT column-average and AIRS mid-tropospheric data. However, the two instruments have different footprints, measurement-error characteristics, and data coverages. In addition, the spatio-temporal domains are large, and the AIRS dataset is massive. In this article, we describe a spatio-temporal data-fusion (STDF) methodology based on reduced-dimensional Kalman smoothing. Our STDF is able to combine the complementary GOSAT and AIRS datasets to optimally estimate lower-atmospheric CO2 mole fraction over the whole globe. Further, it is designed for massive remote sensing datasets and accounts for differences in instrument footprint, measurement-error characteristics, and data coverages. This article has supplementary material online.
C1 [Hai Nguyen; Braverman, Amy] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Katzfuss, Matthias] Heidelberg Univ, Inst Angew Math, D-69117 Heidelberg, Germany.
[Cressie, Noel] Univ Wollongong, Sch Math & Appl Stat, Wollongong, NSW 2522, Australia.
RP Nguyen, H (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM hai.nguyen@jpl.nasa.gov; katzfuss@gmail.com; ncressie@uow.edu.au;
amy.braverman@jpl.nasa.gov
FU NASA's Earth Science Technology Office through its Advanced Information
Systems Technology program; Mathematics Center Heidelberg; Naval Surface
Warfare Center, Dahlgren Division
FX The research described in this article was carried out in part by the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. It is supported by NASA's Earth Science Technology
Office through its Advanced Information Systems Technology program.
Katzfuss' research was partially supported by the Mathematics Center
Heidelberg. Cressie's research was partially supported by the Naval
Surface Warfare Center, Dahlgren Division.
NR 41
TC 3
Z9 3
U1 0
U2 19
PU AMER STATISTICAL ASSOC
PI ALEXANDRIA
PA 732 N WASHINGTON ST, ALEXANDRIA, VA 22314-1943 USA
SN 0040-1706
EI 1537-2723
J9 TECHNOMETRICS
JI Technometrics
PD MAY
PY 2014
VL 56
IS 2
BP 174
EP 185
DI 10.1080/00401706.2013.831774
PG 12
WC Statistics & Probability
SC Mathematics
GA AH2NG
UT WOS:000335957600005
ER
PT J
AU Doarn, CR
Pruitt, S
Jacobs, J
Harris, Y
Bott, DM
Riley, W
Lamer, C
Oliver, AL
AF Doarn, Charles R.
Pruitt, Sherilyn
Jacobs, Jessica
Harris, Yael
Bott, David M.
Riley, William
Lamer, Christopher
Oliver, Anthony L.
TI Original Research Federal Efforts to Define and Advance Telehealth-A
Work in Progress
SO TELEMEDICINE AND E-HEALTH
LA English
DT Article
DE telemedicine; telehealth; U; S; Government; healthcare reform
ID ARMY TELEMEDICINE; MOBILE HEALTH; TECHNOLOGY; FUTURE; CARE;
IMPLEMENTATION; PERSPECTIVES; MANAGEMENT; SUPPORT; HOME
AB Background:The integration of telecommunications and information systems in healthcare is not new or novel; indeed, it is the current practice of medicine and has been an integral part of medicine in remote locations for several decades. The U.S. Government has made a significant investment, measured in hundreds of millions of dollars, and therefore has a strong presence in the integration of telehealth/telemedicine in healthcare. However, the terminologies and definitions in the lexicon vary across agencies and departments of the U.S. Government. The objective of our survey was to identify and evaluate the definitions of telehealth/telemedicine across the U.S. Government to provide a better understanding of what each agency or department means when it uses these terms.Methodology:The U.S. Government, under the leadership of the Health Resources and Services Administration in the U.S. Department of Health and Human Services, established the Federal Telemedicine (FedTel) Working Group, through which all members responded to a survey on each agency or department's definition and use of terms associated with telehealth.Results and Conclusions:Twenty-six agencies represented by more than 100 individuals participating in the FedTel Working Group identified seven unique definitions of telehealth in current use across the U.S. Government. Although many definitions are similar, there are nuanced differences that reflect each organization's legislative intent and the population they serve. These definitions affect how telemedicine has been or is being applied across the healthcare landscape, reflecting the U.S. Government's widespread and influential role in healthcare access and service delivery. The evidence base suggests that a common nomenclature for defining telemedicine may benefit efforts to advance the use of this technology to address the changing nature of healthcare and new demands for services expected as a result of health reform.
C1 [Doarn, Charles R.] NASA Headquarters, Washington, DC USA.
[Doarn, Charles R.] Univ Cincinnati, Coll Med, Dept Family & Community Med, Cincinnati, OH 45267 USA.
[Pruitt, Sherilyn; Oliver, Anthony L.] US Dept HHS, Off Adv Telehlth, Rockville, MD USA.
[Jacobs, Jessica] Aetna, Washington, DC USA.
[Harris, Yael] US Dept HHS, Div Healthcare Qual, Off Dis Prevent & Hlth Promot, Rockville, MD USA.
[Bott, David M.] US Dept HHS, Ctr Medicare & Medicaid Serv, Baltimore, MD USA.
[Riley, William] NCI, Div Canc Control & Populat Sci, Bethesda, MD 20892 USA.
[Lamer, Christopher] Indian Hlth Serv, Rockville, MD USA.
RP Doarn, CR (reprint author), Univ Cincinnati, Coll Med, Dept Family & Community Med, Cincinnati, OH 45267 USA.
EM charles.doarn@uc.edu
NR 36
TC 9
Z9 9
U1 0
U2 5
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1530-5627
EI 1556-3669
J9 TELEMED E-HEALTH
JI Telemed. e-Health
PD MAY 1
PY 2014
VL 20
IS 5
BP 409
EP 418
DI 10.1089/tmj.2013.0336
PG 10
WC Health Care Sciences & Services
SC Health Care Sciences & Services
GA AG4MG
UT WOS:000335393400004
PM 24502793
ER
PT J
AU Comiso, JC
Hall, DK
AF Comiso, Josefino C.
Hall, Dorothy K.
TI Climate trends in the Arctic as observed from space
SO WILEY INTERDISCIPLINARY REVIEWS-CLIMATE CHANGE
LA English
DT Review
ID GREENLAND ICE-SHEET; INTERACTIVE MULTISENSOR SNOW; SEA-SURFACE
TEMPERATURE; NORTHERN-HEMISPHERE; AIR-TEMPERATURE; MASS-LOSS;
SATELLITE-OBSERVATIONS; RADIATION PROPERTIES; MAPPING SYSTEM; LEVEL RISE
AB The Arctic is a region in transformation. Warming in the region has been amplified, as expected from ice-albedo feedback effects, with the rate of warming observed to be approximate to 0.600.07 degrees C/decade in the Arctic (>64 degrees N) compared to approximate to 0.17 degrees C/decade globally during the last three decades. This increase in surface temperature is manifested in all components of the cryosphere. In particular, the sea ice extent has been declining at the rate of approximate to 3.8%/decade, whereas the perennial ice (represented by summer ice minimum) is declining at a much greater rate of approximate to 11.5%/decade. Spring snow cover has also been observed to be declining by -2.12%/decade for the period 1967-2012. The Greenland ice sheet has been losing mass at the rate of approximate to 34.0Gt/year (sea level equivalence of 0.09mm/year) during the period from 1992 to 2011, but for the period 2002-2011, a higher rate of mass loss of approximate to 215Gt/year has been observed. Also, the mass of glaciers worldwide declined at the rate of 226 Gt/year from 1971 to 2009 and 275 Gt/year from 1993 to 2009. Increases in permafrost temperature have also been measured in many parts of the Northern Hemisphere while a thickening of the active layer that overlies permafrost and a thinning of seasonally frozen ground has also been reported. To gain insight into these changes, comparative analysis with trends in clouds, albedo, and the Arctic Oscillation is also presented. For further resources related to this article, please visit the . Conflict of interest: The authors have declared no conflicts of interest for this article.
C1 [Comiso, Josefino C.; Hall, Dorothy K.] NASA, Goddard Space Flight Ctr, Code Earth Sci Div 615, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
RP Comiso, JC (reprint author), NASA, Goddard Space Flight Ctr, Code Earth Sci Div 615, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
EM josefino.c.comiso@nasa.gov
NR 122
TC 47
Z9 50
U1 12
U2 75
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1757-7780
EI 1757-7799
J9 WIRES CLIM CHANGE
JI Wiley Interdiscip. Rev.-Clim. Chang.
PD MAY
PY 2014
VL 5
IS 3
BP 389
EP 409
DI 10.1002/wcc.277
PG 21
WC Environmental Studies; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AF3CQ
UT WOS:000334589500007
ER
PT J
AU Arendt, RG
Dwek, E
Kober, G
Rho, J
Hwang, U
AF Arendt, Richard G.
Dwek, Eli
Kober, Gladys
Rho, Jeonghee
Hwang, Una
TI INTERSTELLAR AND EJECTA DUST IN THE CAS A SUPERNOVA REMNANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust,extinction; infrared: ISM; ISM: individual objects: (Cassiopeia A);
ISM: supernova remnants
ID CASSIOPEIA-A SUPERNOVA; OPTICAL-PROPERTIES; SILICATE MINERALOGY;
INFRARED-EMISSION; 3-DIMENSIONAL STRUCTURE; EARLY UNIVERSE; SPITZER;
CARBON; ORIGIN; GRAINS
AB Infrared continuum observations provide a means of investigating the physical composition of the dust in the ejecta and swept up medium of the Cas A supernova remnant (SNR). Using low-resolution Spitzer IRS spectra (5-35 mu m), and broad-band Herschel PACS imaging (70, 100, and 160 mu m), we identify characteristic dust spectra, associated with ejecta layers that underwent distinct nuclear burning histories. The most luminous spectrum exhibits strong emission features at similar to 9 and 21 mu m and is closely associated with ejecta knots with strong Ar emission lines. The dust features can be reproduced by magnesium silicate grains with relatively low Mg to Si ratios. Another dust spectrum is associated with ejecta having strong Ne emission lines. It has no indication of any silicate features and is best fit by Al2O3 dust. A third characteristic dust spectrum shows features that are best matched by magnesium silicates with a relatively high Mg to Si ratio. This dust is primarily associated with the X-ray-emitting shocked ejecta, but it is also evident in regions where shocked interstellar or circumstellar material is expected. However, the identification of dust composition is not unique, and each spectrum includes an additional featureless dust component of unknown composition. Colder dust of indeterminate composition is associated with emission from the interior of the SNR, where the reverse shock has not yet swept up and heated the ejecta. Most of the dust mass in Cas A is associated with this unidentified cold component, which is less than or similar to 0.1M(circle dot). The mass of warmer dust is only similar to 0.04M(circle dot).
C1 [Arendt, Richard G.] Univ Maryland, CRESST, Baltimore, MD 21250 USA.
[Arendt, Richard G.; Dwek, Eli; Kober, Gladys; Hwang, Una] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kober, Gladys] Catholic Univ Amer, Dept Phys, IACS, Washington, DC 20064 USA.
[Rho, Jeonghee] SETI Inst, Mountain View, CA 94043 USA.
[Rho, Jeonghee] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Hwang, Una] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Arendt, RG (reprint author), Univ Maryland, CRESST, Baltimore, MD 21250 USA.
EM Richard.G.Arendt@nasa.gov
OI Arendt, Richard/0000-0001-8403-8548
FU NASA [NNH09ZDA001N-ADP-0032]
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 Program NNH09ZDA001N-ADP-0032. This
research made use of Tiny Tim/Spitzer, developed by John Krist for the
Spitzer Science Center. The Center is managed by the California
Institute of Technology under a contract with NASA. This research has
made use of NASA ' s Astrophysics Data System Bibliographic Services. We
thank T. Kozasa for providing digitized (and extrapolated and
interpolated) versions of the optical constants for several dust species
as noted in Table 3. We also thank the referee for constructive comments
on the manuscript.
NR 71
TC 17
Z9 17
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 MAY 1
PY 2014
VL 786
IS 1
AR 55
DI 10.1088/0004-637X/786/1/55
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH0LF
UT WOS:000335810700055
ER
PT J
AU Barriere, NM
Tomsick, JA
Baganoff, FK
Boggs, SE
Christensen, FE
Craig, WW
Dexter, J
Grefenstette, B
Hailey, CJ
Harrison, FA
Madsen, KK
Mori, K
Stern, D
Zhang, WW
Zhang, S
Zoglauer, A
AF Barriere, Nicolas M.
Tomsick, John A.
Baganoff, Frederick K.
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Dexter, Jason
Grefenstette, Brian
Hailey, Charles J.
Harrison, Fiona A.
Madsen, Kristin K.
Mori, Kaya
Stern, Daniel
Zhang, William W.
Zhang, Shuo
Zoglauer, Andreas
TI NuSTAR DETECTION OF HIGH-ENERGY X-RAY EMISSION AND RAPID VARIABILITY
FROM SAGITTARIUS A(star) FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; Galaxy: center; stars: black holes; stars:
flare; stars: individual (Sgr A*); X-rays: general
ID SGR-A-ASTERISK; SUPERMASSIVE BLACK-HOLE; NEAR-INFRARED FLARES;
EXTRAGALACTIC RADIO-SOURCES; GALACTIC-CENTER; FLARING ACTIVITY;
XMM-NEWTON; BRIGHTEST FLARE; ACCRETION FLOW; STELLAR ORBITS
AB Sagittarius A(star) harbors the supermassive black hole that lies at the dynamical center of our Galaxy. Sagittarius A(star) spends most of its time in a low luminosity emission state but flares frequently in the infrared and X-ray, increasing up to a few hundred fold in brightness for up to a few hours at a time. The physical processes giving rise to the X-ray flares are uncertain. Here we report the detection with the NuSTAR observatory in Summer and Fall 2012 of four low to medium amplitude X-ray flares to energies up to 79 keV. For the first time, we clearly see that the power-law spectrum of Sagittarius A(star) X-ray flares extends to high energy, with no evidence for a cutoff. Although the photon index of the absorbed power-law fits are in agreement with past observations, we find a difference between the photon index of two of the flares (significant at the 95% confidence level). The spectra of the two brightest flares (similar to 55 times quiescence in the 2-10 keV band) are compared to simple physical models in an attempt to identify the main X-ray emission mechanism, but the data do not allow us to significantly discriminate between them. However, we confirm the previous finding that the parameters obtained with synchrotron models are, for the X-ray emission, physically more reasonable than those obtained with inverse Compton models. One flare exhibits large and rapid (< 100 s) variability, which, considering the total energy radiated, constrains the location of the flaring region to be within similar to 10 Schwarzschild radii of the black hole.
C1 [Barriere, Nicolas M.; Tomsick, John A.; Boggs, Steven E.; Craig, William W.; Zoglauer, Andreas] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Baganoff, Frederick K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[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.
[Dexter, Jason] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Dexter, Jason] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Grefenstette, Brian; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Hailey, Charles J.; Mori, Kaya; Zhang, Shuo] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
RP Barriere, NM (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RI Boggs, Steven/E-4170-2015
OI Boggs, Steven/0000-0001-9567-4224
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration
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). The authors thank S. Nayakshin, S.
Markoff, A. Eckart, G. Trap, M. Wardle, and F. Yusef-Zadeh for useful
discussions. We also thank the Chandra Sgr Astar XVP
collaboration for information on absence of X-ray transients before and
after the flares reported here.
NR 55
TC 27
Z9 27
U1 1
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 MAY 1
PY 2014
VL 786
IS 1
AR 46
DI 10.1088/0004-637X/786/1/46
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH0LF
UT WOS:000335810700046
ER
PT J
AU Brandt, TD
Kuzuhara, M
McElwain, MW
Schlieder, JE
Wisniewski, JP
Turner, EL
Carson, J
Matsuo, T
Biller, B
Bonnefoy, M
Dressing, C
Janson, M
Knapp, GR
Moro-Martin, A
Thalmann, C
Kudo, T
Kusakabe, N
Hashimoto, J
Abe, L
Brandner, W
Currie, T
Egner, S
Feldt, M
Golota, T
Goto, M
Grady, CA
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Kandori, R
Kwon, J
Mede, K
Miyama, S
Morino, JI
Nishimura, T
Pyo, TS
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takami, M
Takahashi, Y
Takato, N
Terada, H
Tomono, D
Watanabe, M
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Brandt, Timothy D.
Kuzuhara, Masayuki
McElwain, Michael W.
Schlieder, Joshua E.
Wisniewski, John P.
Turner, Edwin L.
Carson, J.
Matsuo, T.
Biller, B.
Bonnefoy, M.
Dressing, C.
Janson, M.
Knapp, G. R.
Moro-Martin, A.
Thalmann, C.
Kudo, T.
Kusakabe, N.
Hashimoto, J.
Abe, L.
Brandner, W.
Currie, T.
Egner, S.
Feldt, M.
Golota, T.
Goto, M.
Grady, C. A.
Guyon, O.
Hayano, Y.
Hayashi, M.
Hayashi, S.
Henning, T.
Hodapp, K. W.
Ishii, M.
Iye, M.
Kandori, R.
Kwon, J.
Mede, K.
Miyama, S.
Morino, J. -I.
Nishimura, T.
Pyo, T. -S.
Serabyn, E.
Suenaga, T.
Suto, H.
Suzuki, R.
Takami, M.
Takahashi, Y.
Takato, N.
Terada, H.
Tomono, D.
Watanabe, M.
Yamada, T.
Takami, H.
Usuda, T.
Tamura, M.
TI THE MOVING GROUP TARGETS OF THE SEEDS HIGH-CONTRAST IMAGING SURVEY OF
EXOPLANETS AND DISKS: RESULTS AND OBSERVATIONS FROM THE FIRST THREE
YEARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; brown dwarfs; open clusters and associations: general;
stars: activity; stars: imaging; stars: low-mass; stars: planetary
systems
ID TW-HYDRAE ASSOCIATION; LATE-TYPE STARS; LOW-MASS STARS; MAIN-SEQUENCE
STARS; STELLAR KINEMATIC GROUPS; YOUNG SOLAR ANALOGS; ALL-SKY SURVEY;
EXTRASOLAR GIANT PLANETS; GENEVA-COPENHAGEN SURVEY; ADAPTIVE OPTICS
SURVEY
AB We present results from the first three years of observations of moving group (MG) targets in the Strategic Exploration of Exoplanets and Disks with Subaru (SEEDS) high-contrast imaging survey of exoplanets and disks using the Subaru telescope. We achieve typical contrasts of similar to 10(5) at 1 '' and similar to 10(6) beyond 2 '' around 63 proposed members of nearby kinematic MGs. We review each of the kinematic associations to which our targets belong, concluding that five, beta Pictoris (similar to 20 Myr), AB Doradus (similar to 100 Myr), Columba (similar to 30 Myr), Tucana-Horogium (similar to 30 Myr), and TW Hydrae (similar to 10 Myr), are sufficiently well-defined to constrain the ages of individual targets. Somewhat less than half of our targets are high-probability members of one of these MGs. For all of our targets, we combine proposed MG membership with other age indicators where available, including Ca II HK emission, X-ray activity, and rotation period, to produce a posterior probability distribution of age. SEEDS observations discovered a substellar companion to one of our targets,. And, a late B star. We do not detect any other substellar companions, but do find seven new close binary systems, of which one still needs to be confirmed. A detailed analysis of the statistics of this sample, and of the companion mass constraints given our age probability distributions and exoplanet cooling models, will be presented in a forthcoming paper.
C1 [Brandt, Timothy D.; Turner, Edwin L.; Janson, M.; Knapp, G. R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kuzuhara, Masayuki] Tokyo Inst Technol, Tokyo 152, Japan.
[McElwain, Michael W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Schlieder, Joshua E.; Carson, J.; Biller, B.; Bonnefoy, M.; Brandner, W.; Feldt, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Matsuo, T.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Univ WPI, Tokyo 1138654, Japan.
[Carson, J.] Coll Charleston, Charleston, SC 29401 USA.
[Matsuo, T.] Kyoto Univ, Dept Astron, Kyoto, Japan.
[Dressing, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Moro-Martin, A.] CAB CSIC INTA, Dept Astrophys, Madrid, Spain.
[Thalmann, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands.
[Kudo, T.; Egner, S.; Golota, T.; 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 USA.
[Kusakabe, N.; Hashimoto, J.; Iye, M.; Kandori, R.; Kwon, J.; Morino, J. -I.; Suto, H.; Suzuki, R.; Tamura, M.] Natl Astron Observ Japan, Tokyo, Japan.
[Abe, L.] Lab Hippolyte Fizeau, Nice, France.
[Currie, T.] Univ Toronto, Toronto, ON, Canada.
[Goto, M.] Univ Sternwarte, Munich, Germany.
[Grady, C. A.] Eureka Sci, Oakland, CA USA.
[Hayashi, M.; Takahashi, Y.; Tamura, M.] Univ Tokyo, Tokyo, Japan.
[Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Kwon, J.; Suenaga, T.] Grad Univ Adv Studies, Dept Astron Sci, Tokyo, Japan.
[Miyama, S.] Hiroshima Univ, Higashihiroshima 724, Japan.
[Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido, Japan.
[Yamada, T.] Tohoku Univ, Astron Inst, Sendai, Miyagi 980, Japan.
RP Brandt, TD (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
NR 237
TC 27
Z9 27
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 MAY 1
PY 2014
VL 786
IS 1
AR 1
DI 10.1088/0004-637X/786/1/1
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH0LF
UT WOS:000335810700001
ER
PT J
AU Broekhoven-Fiene, H
Matthews, BC
Harvey, PM
Gutermuth, RA
Huard, TL
Tothill, NFH
Nutter, D
Bourke, TL
DiFrancesco, J
Jorgensen, JK
Allen, LE
Chapman, NL
Dunham, MM
Merin, B
Miller, JF
Terebey, S
Peterson, DE
Stapelfeldt, KR
AF Broekhoven-Fiene, Hannah
Matthews, Brenda C.
Harvey, Paul M.
Gutermuth, Robert A.
Huard, Tracy L.
Tothill, Nicholas F. H.
Nutter, David
Bourke, Tyler L.
DiFrancesco, James
Jorgensen, Jes K.
Allen, Lori E.
Chapman, Nicholas L.
Dunham, Michael M.
Merin, Bruno
Miller, Jennifer F.
Terebey, Susan
Peterson, Dawn E.
Stapelfeldt, Karl R.
TI THE Spitzer SURVEY OF INTERSTELLAR CLOUDS IN THE GOULD BELT. VI. THE
AURIGA-CALIFORNIA MOLECULAR CLOUD OBSERVED WITH IRAC AND MIPS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: general; ISM: clouds; stars: formation
ID YOUNG STELLAR OBJECTS; ARRAY CAMERA IRAC; T-TAURI STARS; C2D SURVEY;
SPACE-TELESCOPE; NEARBY; PERSEUS; POPULATION; DISTRIBUTIONS;
LUMINOSITIES
AB We present observations of the Auriga-California Molecular Cloud (AMC) at 3.6, 4.5, 5.8, 8.0, 24, 70, and 160 mu m observed with the IRAC and MIPS detectors as part of the Spitzer Gould Belt Legacy Survey. The total mapped areas are 2.5 deg(2) with IRAC and 10.47 deg(2) with MIPS. This giant molecular cloud is one of two in the nearby Gould Belt of star-forming regions, the other being the Orion A Molecular Cloud (OMC). We compare source counts, colors, and magnitudes in our observed region to a subset of the SWIRE data that was processed through our pipeline. Using color-magnitude and color-color diagrams, we find evidence for a substantial population of 166 young stellar objects (YSOs) in the cloud, many of which were previously unknown. Most of this population is concentrated around the LkH alpha 101 cluster and the filament extending from it. We present a quantitative description of the degree of clustering and discuss the relative fraction of YSOs in earlier (Class I and F) and later (Class II) classes compared to other clouds. We perform simple SED modeling of the YSOs with disks to compare the mid-IR properties to disks in other clouds and identify 14 classical transition disk candidates. Although the AMC is similar in mass, size, and distance to the OMC, it is forming about 15-20 times fewer stars.
C1 [Broekhoven-Fiene, Hannah; Matthews, Brenda C.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada.
[Matthews, Brenda C.; DiFrancesco, James] Natl Res Council Herzberg Astron Astrophys, Victoria, BC V9E 2E7, Canada.
[Harvey, Paul M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Gutermuth, Robert A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Huard, Tracy L.; Miller, Jennifer F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Huard, Tracy L.] Univ Western Sydney, Sch Comp Engn & Math, Penrith, NSW 2751, Australia.
[Tothill, Nicholas F. H.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Nutter, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bourke, Tyler L.; Miller, Jennifer F.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark.
[Jorgensen, Jes K.] Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark.
[Jorgensen, Jes K.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Allen, Lori E.] Northwestern Univ, CIERA, Evanston, IL 60208 USA.
[Chapman, Nicholas L.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Chapman, Nicholas L.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Dunham, Michael M.] ESAC ESA, Herschel Sci Ctr, E-28691 Madrid, Spain.
[Merin, Bruno] Space Sci Inst, Boulder, CO 80301 USA.
[Terebey, Susan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Broekhoven-Fiene, H (reprint author), Univ Victoria, Dept Phys & Astron, POB 3055, Victoria, BC V8W 3P6, Canada.
RI Tothill, Nicholas/M-6379-2016
OI Tothill, Nicholas/0000-0002-9931-5162
FU NSERC Discovery Grant; NASA - California Institute of Technology
[NCC5-626]
FX We thank the referee whose comments and suggestions greatly helped
improve the paper and its clarity. H.B.F. gratefully acknowledges
research support from an NSERC Discovery Grant. This research made use
of APLpy, an open-source plotting package for Python hosted at
http://aplpy. github. com. This research also made use of Montage,
funded by the National Aeronautics and Space Administration's Earth
Science Technology Office, Computation Technologies Project, under
Cooperative Agreement Number NCC5-626 between NASA and the California
Institute of Technology. Montage is maintained by the NASA/IPAC Infrared
Science Archive.
NR 39
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U1 0
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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 MAY 1
PY 2014
VL 786
IS 1
AR 37
DI 10.1088/0004-637X/786/1/37
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH0LF
UT WOS:000335810700037
ER
PT J
AU Del Moro, A
Mullaney, JR
Alexander, DM
Comastri, A
Bauer, FE
Treister, E
Stern, D
Civano, F
Ranalli, P
Vignali, C
Aird, JA
Ballantyne, DR
Balokovic, M
Boggs, SE
Brandt, WN
Christensen, FE
Craig, WW
Gandhi, P
Gilli, R
Hailey, CJ
Harrison, FA
Hickox, RC
LaMassa, SM
Lansbury, GB
Luo, B
Puccetti, S
Urry, M
Zhang, WW
AF Del Moro, A.
Mullaney, J. R.
Alexander, D. M.
Comastri, A.
Bauer, F. E.
Treister, E.
Stern, D.
Civano, F.
Ranalli, P.
Vignali, C.
Aird, J. A.
Ballantyne, D. R.
Balokovic, M.
Boggs, S. E.
Brandt, W. N.
Christensen, F. E.
Craig, W. W.
Gandhi, P.
Gilli, R.
Hailey, C. J.
Harrison, F. A.
Hickox, R. C.
LaMassa, S. M.
Lansbury, G. B.
Luo, B.
Puccetti, S.
Urry, M.
Zhang, W. W.
TI NuSTAR J033202-2746.8: DIRECT CONSTRAINTS ON THE COMPTON REFLECTION IN A
HEAVILY OBSCURED QUASAR AT z approximate to 2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; infrared: galaxies; quasars: general; quasars:
individual (NuSTAR J033202-2746.8); X-rays: galaxies
ID DEEP FIELD-SOUTH; ACTIVE GALACTIC NUCLEI; RAY SPECTRAL PROPERTIES; HARD
X-RAYS; XMM-NEWTON OBSERVATIONS; STAR-FORMING GALAXIES; POINT-SOURCE
CATALOGS; LINE RADIO GALAXIES; MS SOURCE CATALOGS; SWIFT-BAT SURVEY
AB We report Nuclear Spectroscopic Telescope Array (NuSTAR) observations of NuSTAR J033202-2746.8, a heavily obscured, radio-loud quasar detected in the Extended Chandra Deep Field-South, the deepest layer of the NuSTAR extragalactic survey (similar to 400 ks, at its deepest). NuSTAR J033202-2746.8 is reliably detected by NuSTAR only at E > 8 keV and has a very flat spectral slope in the NuSTAR energy band (Gamma = 0.55(-0.64)(+0.62); 3-30 keV). Combining the NuSTAR data with extremely deep observations by Chandra and XMM-Newton (4 Ms and 3 Ms, respectively), we constrain the broad-band X-ray spectrum of NuSTAR J033202-2746.8, indicating that this source is a heavily obscured quasar (N-H = 5.6(-0.8)(+0.9) x 10(23) cm(-2)) with luminosity L10-40 keV approximate to 6.4 x 10(44) erg s(-1). Although existing optical and near-infrared (near-IR) data, as well as follow-up spectroscopy with the Keck and VLT telescopes, failed to provide a secure redshift identification for NuSTAR J033202-2746.8, we reliably constrain the redshift z = 2.00 +/- 0.04 from the X-ray spectral features (primarily from the iron K edge). The NuSTAR spectrum shows a significant reflection component (R = 0.55(-0.37)(+0.44)), which was not constrained by previous analyses of Chandra and XMM-Newton data alone. The measured reflection fraction is higher than the R similar to 0 typically observed in bright radio-loud quasars such as NuSTAR J033202-2746.8, which has L-1.4 GHz approximate to 10(27) W Hz(-1). Constraining the spectral shape of active galactic nuclei (AGNs), including bright quasars, is very important for understanding the AGN population, and can have a strong impact on the modeling of the X-ray background. Our results show the importance of NuSTAR in investigating the broad-band spectral properties of quasars out to high redshift.
C1 [Del Moro, A.; Mullaney, J. R.; Alexander, D. M.; Aird, J. A.; Gandhi, P.; Lansbury, G. B.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Mullaney, J. R.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England.
[Comastri, A.; Vignali, C.; Gilli, R.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Civano, F.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA.
[Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ranalli, P.] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, Inst Astron, Penteli 15236, Greece.
[Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy.
[Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Balokovic, M.; Harrison, F. A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 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.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[LaMassa, S. M.; Urry, M.] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA.
[Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Puccetti, S.] INAF Osservatorio Astronomico Roma, I-00040 Monte Porzio Catone, Italy.
[Zhang, W. W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Del Moro, A (reprint author), Univ Durham, Dept Phys, S Rd, Durham DH1 3LE, England.
EM agnese.del-moro@durham.ac.uk
RI Ranalli, Piero/K-6363-2013; Vignali, Cristian/J-4974-2012; Boggs,
Steven/E-4170-2015; Brandt, William/N-2844-2015; Comastri,
Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015;
OI Ranalli, Piero/0000-0003-3956-755X; Vignali,
Cristian/0000-0002-8853-9611; Boggs, Steven/0000-0001-9567-4224; Brandt,
William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970;
Gilli, Roberto/0000-0001-8121-6177; Alexander, David/0000-0002-5896-6313
FU UK Science and Technology Facilities Council (STFC) [ST/I001573/I,
ST/K501979/1, ST/J003697/1]; Leverhulme Trust; ASI/INAF
[I/037/12/0-011/13]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT
1101024]; Anillo [ACT1101]; FONDECYT [1120061]; Caltech NuSTAR
[44A-1092750]; NASA ADP [NNX10AC99G]; NASA [NNG08FD60C]; National
Aeronautics and Space Administration; ESO Telescopes at the La Silla
Paranal Observatory under the program [ID 092.A-0452]
FX We thank the anonymous referee for careful reading and for the helpful
comments, which helped improving this manuscript. We gratefully
acknowledge financial support from the UK Science and Technology
Facilities Council (STFC, ST/I001573/I, ADM and DMA; ST/K501979/1, GBL;
ST/J003697/1, PG) and the Leverhulme Trust (D.M.A. and J.R.M.). A.C.,
C.V., R.G., and P.R. thank the ASI/INAF grant I/037/12/0-011/13. F.E.B.
acknowledges support from Basal-CATA (PFB-06/2007) and CONICYT-Chile
(FONDECYT 1101024 and Anillo grant ACT1101) and E.T. acknowledges the
FONDECYT grant 1120061. W.N.B. and B.L. thank Caltech NuSTAR subcontract
44A-1092750 and NASA ADP grant NNX10AC99G. M.B. acknowledges the
International Fulbright Science and Technology Award. 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). This work also used observations made with ESO
Telescopes at the La Silla Paranal Observatory under the program ID
092.A-0452.
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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 MAY 1
PY 2014
VL 786
IS 1
AR 16
DI 10.1088/0004-637X/786/1/16
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH0LF
UT WOS:000335810700016
ER
PT J
AU Grillo, C
Gobat, R
Presotto, V
Balestra, I
Mercurio, A
Rosati, P
Nonino, M
Vanzella, E
Christensen, L
Graves, G
Biviano, A
Lemze, D
Bartelmann, M
Benitez, N
Bouwens, R
Bradley, L
Broadhurst, T
Coe, D
Donahue, M
Ford, H
Infante, L
Jouvel, S
Kelson, D
Koekemoer, A
Lahav, O
Medezinski, E
Melchior, P
Meneghetti, M
Merten, J
Molino, A
Monna, A
Moustakas, J
Moustakas, LA
Postman, M
Seitz, S
Umetsu, K
Zheng, W
Zitrin, A
AF Grillo, C.
Gobat, R.
Presotto, V.
Balestra, I.
Mercurio, A.
Rosati, P.
Nonino, M.
Vanzella, E.
Christensen, L.
Graves, G.
Biviano, A.
Lemze, D.
Bartelmann, M.
Benitez, N.
Bouwens, R.
Bradley, L.
Broadhurst, T.
Coe, D.
Donahue, M.
Ford, H.
Infante, L.
Jouvel, S.
Kelson, D.
Koekemoer, A.
Lahav, O.
Medezinski, E.
Melchior, P.
Meneghetti, M.
Merten, J.
Molino, A.
Monna, A.
Moustakas, J.
Moustakas, L. A.
Postman, M.
Seitz, S.
Umetsu, K.
Zheng, W.
Zitrin, A.
TI CLASH: EXTENDING GALAXY STRONG LENSING TO SMALL PHYSICAL SCALES WITH
DISTANT SOURCES HIGHLY MAGNIFIED BY GALAXY CLUSTER MEMBERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; galaxies: clusters: individual (MACS J1206.2-0847);
galaxies: high-redshift; galaxies: stellar content; galaxies: structure;
gravitational lensing: strong
ID INITIAL MASS FUNCTION; SPECTROSCOPICALLY SELECTED SAMPLE; DARK-MATTER
HALOS; ACS SURVEY; GRAVITATIONAL LENSES; ADVANCED CAMERA; 2-DIMENSIONAL
KINEMATICS; INTERNAL STRUCTURE; MACS J1206.2-0847; RXC J2248.7-4431
AB We present a complex strong lensing system in which a double source is imaged five times by two early-type galaxies. We take advantage in this target of the extraordinary multi-band photometric data set obtained as part of the Cluster Lensing And Supernova survey with Hubble (CLASH) program, complemented by the spectroscopic measurements of the VLT/VIMOS and FORS2 follow-up campaign. We use a photometric redshift value of 3.7 for the source and confirm spectroscopically the membership of the two lenses to the galaxy cluster MACS J1206.2-0847 at redshift 0.44. We exploit the excellent angular resolution of the HST/ACS images to model the two lenses in terms of singular isothermal sphere profiles and derive robust effective velocity dispersion values of 97 +/- 3 and 240 +/- 6 km s(-1). Interestingly, the total mass distribution of the cluster is also well characterized by using only the local information contained in this lensing system, which is located at a projected distance of more than 300 kpc from the cluster luminosity center. According to our best-fitting lensing and composite stellar population models, the source is magnified by a total factor of 50 and has a luminous mass of approximately (1.0 +/- 0.5) x10(9) M circle dot (assuming a Salpeter stellar initial mass function). By combining the total and luminous mass estimates of the two lenses, we measure luminous over total mass fractions projected within the effective radii of 0.51 +/- 0.21 and 0.80 +/- 0.32. Remarkably, with these lenses we can extend the analysis of the mass properties of lens early-type galaxies by factors that are approximately two and three times smaller than previously done with regard to, respectively, velocity dispersion and luminous mass. The comparison of the total and luminous quantities of our lenses with those of astrophysical objects with different physical scales, like massive early-type galaxies and dwarf spheroidals, reveals the potential of studies of this kind for improving our knowledge about the internal structure of galaxies. These studies, made possible thanks to the CLASH survey, will allow us to go beyond the current limits posed by the available lens samples in the field.
C1 [Grillo, C.; Christensen, L.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Gobat, R.] Univ Paris Diderot, CEA Saclay, CEA DSM CNRS, Irfu Serv Astrophys,Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France.
[Presotto, V.] Univ Trieste, Dipartimento Fis, I-34143 Trieste, Italy.
[Balestra, I.; Nonino, M.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Balestra, I.; Mercurio, A.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Rosati, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy.
[Vanzella, E.; Meneghetti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Graves, G.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Lemze, D.; Medezinski, E.; Zheng, W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Bartelmann, M.] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Benitez, N.; Molino, A.] CSIC, Inst Astrofis Andalucia, Granada 18008, Spain.
[Bouwens, R.] Leiden Univ, Leiden Observ, NL-2333 Leiden, Netherlands.
[Bradley, L.; Coe, D.; Koekemoer, A.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21208 USA.
[Broadhurst, T.] Univ Basque Country, Dept Theoret Phys, E-48080 Bilbao, Spain.
[Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Infante, L.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Jouvel, S.] CSIC, IEE, Inst Cincies Espai, Bellaterra 08193, Barcelona, Spain.
[Jouvel, S.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Melchior, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Merten, J.; Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Monna, A.; Seitz, S.] Univ Sternwarte, Inst Astron & Astrophys, D-81679 Munich, Germany.
[Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA.
[Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Zitrin, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RP Grillo, C (reprint author), Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark.
EM grillo@dark-cosmology.dk
RI Christensen, Lise/M-5301-2014; Grillo, Claudio/E-6223-2015; Meneghetti,
Massimo/O-8139-2015;
OI Koekemoer, Anton/0000-0002-6610-2048; Benitez,
Narciso/0000-0002-0403-7455; Christensen, Lise/0000-0001-8415-7547;
Grillo, Claudio/0000-0002-5926-7143; Meneghetti,
Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662;
Moustakas, Leonidas/0000-0003-3030-2360; Balestra,
Italo/0000-0001-9660-894X; Vanzella, Eros/0000-0002-5057-135X; Umetsu,
Keiichi/0000-0002-7196-4822; Biviano, Andrea/0000-0002-0857-0732
FU Association of Universities for Research in Astronomy, Inc., under NASA
[NAS 5-26555]; NASA [NAS 5-32864, HST-GO-12065.01-A]; DNRF; DFG Cluster
of Excellence Origin Structure of the Universe; PRIN INAF;
Cofinanziamento di Ateneo; NASA through Hubble Fellowship
[HST-HF-51334.01-A]; STScI; "Internationale Spitzenforschung II/2-6" of
the Baden Wurttemberg Stiftung
FX The CLASH Multi-Cycle Treasury Program 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. ACS was developed
under NASA Contract NAS 5-32864. This research is supported in part by
NASA grant HST-GO-12065.01-A. We thank ESO for the continuous support of
the Large Programme 186.A-0798. The Dark Cosmology Centre is funded by
the DNRF. We acknowledge partial support by the DFG Cluster of
Excellence Origin Structure of the Universe. V.P. acknowledges the grant
PRIN INAF 2010 and "Cofinanziamento di Ateneo 2010." The work of L.A.M.
was carried out at Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. Support for A.Z. is provided by
NASA through Hubble Fellowship grant HST-HF-51334.01-A awarded by STScI.
Part of this work was also supported by contract research
"Internationale Spitzenforschung II/2-6" of the Baden Wurttemberg
Stiftung.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
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VL 786
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AR 11
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PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH0LF
UT WOS:000335810700011
ER
PT J
AU Hagen, A
Ciardullo, R
Gronwall, C
Acquaviva, V
Bridge, J
Zeimann, GR
Blanc, GA
Bond, NA
Finkelstein, SL
Song, M
Gawiser, E
Fox, DB
Gebhardt, H
Malz, AI
Schneider, DP
Drory, N
Gebhardt, K
Hill, GJ
AF Hagen, Alex
Ciardullo, Robin
Gronwall, Caryl
Acquaviva, Viviana
Bridge, Joanna
Zeimann, Gregory R.
Blanc, Guillermo A.
Bond, Nicholas A.
Finkelstein, Steven L.
Song, Mimi
Gawiser, Eric
Fox, Derek B.
Gebhardt, Henry
Malz, A. I.
Schneider, Donald P.
Drory, Niv
Gebhardt, Karl
Hill, Gary J.
TI SPECTRAL ENERGY DISTRIBUTION FITTING OF HETDEX PILOT SURVEY Ly alpha
EMITTERS IN COSMOS AND GOODS-N
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: evolution; galaxies: high-redshift;
galaxies: starburst
ID LYMAN BREAK GALAXIES; STAR-FORMATION HISTORIES; EMISSION-LINE GALAXIES;
HIGH-REDSHIFT GALAXIES; EXTRAGALACTIC LEGACY SURVEY; INITIAL MASS
FUNCTION; EMITTING GALAXIES; STELLAR MASS; MORPHOLOGICAL PROPERTIES;
SUBMILLIMETER GALAXIES
AB We use broadband photometry extending from the rest-frame UV to the near-IR to fit the individual spectral energy distributions of 63 bright (L(Ly alpha) > 10(43) erg s(-1)) Ly alpha emitting galaxies (LAEs) in the redshift range 1.9 < z < 3.6. We find that these LAEs are quite heterogeneous, with stellar masses that span over three orders of magnitude, from 7.5 < log M/M-circle dot < 10.5. Moreover, although most LAEs have small amounts of extinction, some high-mass objects have stellar reddenings as large as E(B - V) similar to 0.4. Interestingly, in dusty objects the optical depths for Ly alpha and the UV continuum are always similar, indicating that Ly alpha photons are not undergoing many scatters before escaping their galaxy. In contrast, the ratio of optical depths in low-reddening systems can vary widely, illustrating the diverse nature of the systems. Finally, we show that in the star-formation-rate-log-mass diagram, our LAEs fall above the "main-sequence" defined by z similar to 3 continuum selected star-forming galaxies. In this respect, they are similar to submillimeter-selected galaxies, although most LAEs have much lower mass.
C1 [Hagen, Alex; Ciardullo, Robin; Gronwall, Caryl; Bridge, Joanna; Zeimann, Gregory R.; Fox, Derek B.; Gebhardt, Henry; Malz, A. I.; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Acquaviva, Viviana] CUNY, New York City Coll Technol, Dept Phys, Brooklyn, NY 11201 USA.
[Blanc, Guillermo A.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Bond, Nicholas A.] NASA, Goddard Space Flight Ctr, Cosmol Lab, Greenbelt, MD 20771 USA.
[Finkelstein, Steven L.; Song, Mimi; Drory, Niv; Gebhardt, Karl; Hill, Gary J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Hagen, Alex; Ciardullo, Robin; Gronwall, Caryl; Bridge, Joanna; Zeimann, Gregory R.; Fox, Derek B.; Gebhardt, Henry; Malz, A. I.; Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
RP Hagen, A (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM hagen@psu.edu; rbc@astro.psu.edu; caryl@astro.psu.edu;
vacquaviva@citytech.cuny.edu; jsbridge@psu.edu; grzeimann@psu.edu;
gblancm@obs.carnegiescience.edu; nicholas.bond@nasa.gov;
stevenf@astro.as.utexas.edu; mmsong@astro.as.utexas.edu;
drory@astro.as.utexas.edu; dfox@astro.psu.edu; gebhardt@psu.edu;
malz@psu.edu; dps@astro.psu.edu; drory@astro.as.utexas.edu;
gebhardt@astro.as.utexas.edu; hill@astro.as.utexas.edu
RI Blanc, Guillermo/I-5260-2016;
OI Hagen, Alex/0000-0003-2031-7737
FU NASA [NAS5-26555]; NSF [AST 09-26641, AST 10-55919]; Eberly College of
Science; Office of the Senior Vice President for Research at the
Pennsylvania State University
FX We thank the referee for helpful comments. We also thank Joshua Adams
for the use of his photometry from the HET-DEX Pilot Survey. We
acknowledge the Research Computer and Cyberinfrastructure Unit of
Information Technology Services, and in particular W. Brouwer at The
Pennsylvania State University for providing computational support and
resources for this project. This work is based on observations taken by
the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS5-26555. The work was also partially
supported by NSF grants AST 09-26641 and AST 10-55919. 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.
NR 87
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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 MAY 1
PY 2014
VL 786
IS 1
AR 59
DI 10.1088/0004-637X/786/1/59
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH0LF
UT WOS:000335810700059
ER
PT J
AU Hoard, DW
Long, KS
Howell, SB
Wachter, S
Brinkworth, CS
Knigge, C
Drew, JE
Szkody, P
Kafka, S
Belle, K
Ciardi, DR
Froning, CS
van Belle, GT
Pretorius, ML
AF Hoard, D. W.
Long, Knox S.
Howell, Steve B.
Wachter, Stefanie
Brinkworth, Carolyn S.
Knigge, Christian
Drew, J. E.
Szkody, Paula
Kafka, S.
Belle, Kunegunda
Ciardi, David R.
Froning, Cynthia S.
van Belle, Gerard T.
Pretorius, M. L.
TI NOVA-LIKE CATACLYSMIC VARIABLES IN THE INFRARED
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion; accretion disks; circumstellar matter; infrared: stars;
novae, cataclysmic variables; stars: individual (TT Ari, WX Ari, QU Car,
V592 Cas, V442 Oph, V347 Pup, V3885 Sgr, VY Scl, RW Sex, RW Tri, UX UMa,
IX Vel)
ID UX URSAE MAJORIS; SW SEXTANTIS STAR; SPITZER-SPACE-TELESCOPE;
CIRCUMBINARY ENVELOPE FORMATION; AQUARII PLANETARY SYSTEM; VY SCL STARS;
ACCRETION DISK; TT-ARIETIS; WHITE-DWARF; X-RAY
AB Nova-like (NL) cataclysmic variables have persistently high mass transfer rates and prominent steady state accretion disks. We present an analysis of infrared observations of 12 NLs obtained from the Two Micron All Sky Survey, the Spitzer Space Telescope, and the Wide-field Infrared Survey Explorer All Sky Survey. The presence of an infrared excess at lambda greater than or similar to 3-5 mu m over the expectation of a theoretical steady state accretion disk is ubiquitous in our sample. The strength of the infrared excess is not correlated with orbital period, but shows a statistically significant correlation (but shallow trend) with system inclination that might be partially (but not completely) linked to the increasing view of the cooler outer accretion disk and disk rim at higher inclinations. We discuss the possible origin of the infrared excess in terms of emission from bremsstrahlung or circumbinary dust, with either mechanism facilitated by the mass outflows (e.g., disk wind/corona, accretion stream overflow, and so on) present in NLs. Our comparison of the relative advantages and disadvantages of either mechanism for explaining the observations suggests that the situation is rather ambiguous, largely circumstantial, and in need of stricter observational constraints.
C1 [Hoard, D. W.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Hoard, D. W.; Wachter, Stefanie] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Brinkworth, Carolyn S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Brinkworth, Carolyn S.; Ciardi, David R.] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Knigge, Christian] Univ Southampton, Southampton, Hants, England.
[Drew, J. E.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Szkody, Paula] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Kafka, S.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
[Belle, Kunegunda] Los Alamos Natl Lab, Los Alamos, NM USA.
[Froning, Cynthia S.] Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[van Belle, Gerard T.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Pretorius, M. L.] Univ Oxford, Dept Phys, Oxford, England.
RP Hoard, DW (reprint author), Eureka Sci Inc, Oakland, CA 94602 USA.
EM hoard@mpia.de
OI Ciardi, David/0000-0002-5741-3047; Drew, Janet/0000-0003-1192-7082;
Long, Knox/0000-0002-4134-864X
FU NASA; National Science Foundation (NSF)
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory (JPL),
California Institute of Technology (Caltech), under a contract with the
National Aeronautics and Space Administration (NASA). Support for this
work was provided by NASA. We acknowledge with thanks the variable star
observations from the AAVSO International Database contributed by
observers worldwide and used in this research. This work is also based
on data, data products, and other resources obtained from: (1) The Two
Micron All Sky Survey (2MASS), a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center
(IPAC)/Caltech, funded by NASA and the National Science Foundation
(NSF). (2) NASA's Astrophysics Data System. (3) The NASA/IPAC Infrared
Science Archive (IRSA), which is operated by JPL/Caltech, under a
contract with NASA. (4) The SIMBAD database, operated at CDS,
Strasbourg, France. (5) The Wide-field Infrared Survey Explorer (WISE),
which is a joint project of the University of California, Los Angeles,
and JPL/Caltech, funded by NASA.
NR 201
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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 MAY 1
PY 2014
VL 786
IS 1
AR 68
DI 10.1088/0004-637X/786/1/68
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH0LF
UT WOS:000335810700068
ER
PT J
AU Patel, B
McCully, C
Jha, SW
Rodney, SA
Jones, DO
Graur, OR
Merten, J
Zitrin, A
Riess, AG
Matheson, T
Sako, M
Holoien, TWS
Postman, M
Coe, D
Bartelmann, M
Balestra, I
Benitez, N
Bouwens, R
Bradley, L
Broadhurst, T
Cenko, SB
Donahue, M
Filippenko, AV
Ford, H
Garnavich, P
Grillo, C
Infante, L
Jouvel, S
Kelson, D
Koekemoer, A
Lahav, O
Lemze, D
Maoz, D
Medezinski, E
Melchior, P
Meneghetti, M
Molino, A
Moustakas, J
Moustakas, LA
Nonino, M
Rosati, P
Seitz, S
Strolger, LG
Umetsu, K
Zheng, W
AF Patel, Brandon
McCully, Curtis
Jha, Saurabh W.
Rodney, Steven A.
Jones, David O.
Graur, O. R.
Merten, Julian
Zitrin, Adi
Riess, Adam G.
Matheson, Thomas
Sako, Masao
Holoien, Thomas W. -S.
Postman, Marc
Coe, Dan
Bartelmann, Matthias
Balestra, Italo
Benitez, Narciso
Bouwens, Rychard
Bradley, Larry
Broadhurst, Tom
Cenko, S. Bradley
Donahue, Megan
Filippenko, Alexei V.
Ford, Holland
Garnavich, Peter
Grillo, Claudio
Infante, Leopoldo
Jouvel, Stephanie
Kelson, Daniel
Koekemoer, Anton
Lahav, Ofer
Lemze, Doron
Maoz, Dan
Medezinski, Elinor
Melchior, Peter
Meneghetti, Massimo
Molino, Alberto
Moustakas, John
Moustakas, Leonidas A.
Nonino, Mario
Rosati, Piero
Seitz, Stella
Strolger, Louis G.
Umetsu, Keiichi
Zheng, Wei
TI THREE GRAVITATIONALLY LENSED SUPERNOVAE BEHIND CLASH GALAXY CLUSTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: clusters: general; gravitational
lensing: weak; supernovae: general
ID DIGITAL SKY SURVEY; HIGH-REDSHIFT SUPERNOVAE; HUBBLE-SPACE-TELESCOPE; IA
LIGHT CURVES; FARTHEST KNOWN SUPERNOVA; DARK-ENERGY CONSTRAINTS; LEGACY
SURVEY; DISTANT SUPERNOVAE; COSMOLOGICAL PARAMETERS; ACCELERATING
UNIVERSE
AB We report observations of three gravitationally lensed supernovae (SNe) in the Cluster Lensing And Supernova survey with Hubble (CLASH) Multi-Cycle Treasury program. These objects, SN CLO12Car (z = 1.28), SN CLN12Did (z = 0.85), and SN CLA11Tib (z = 1.14), are located behind three different clusters, MACSJ1720.2+3536 (z = 0.391), RXJ1532.9+3021 (z = 0.345), and A383 (z = 0.187), respectively. Each SN was detected in Hubble Space Telescope optical and infrared images. Based on photometric classification, we find that SNe CLO12Car and CLN12Did are likely to be Type Ia supernovae (SNe Ia), while the classification of SN CLA11Tib is inconclusive. Using multi-color light-curve fits to determine a standardized SN Ia luminosity distance, we infer that SN CLO12Car was similar to 1.0 +/- 0.2 mag brighter than field SNe Ia at a similar redshift and ascribe this to gravitational lens magnification. Similarly, SN CLN12Did is similar to 0.2 +/- 0.2 mag brighter than field SNe Ia. We derive independent estimates of the predicted magnification from CLASH strong+weak-lensing maps of the clusters (in magnitude units, 2.5 log(10) mu): 0.83 +/- 0.16 mag for SN CLO12Car, 0.28 +/- 0.08 mag for SN CLN12Did, and 0.43 +/- 0.11 mag for SN CLA11Tib. The two SNe Ia provide a new test of the cluster lens model predictions: we find that the magnifications based on the SN Ia brightness and those predicted by the lens maps are consistent. Our results herald the promise of future observations of samples of cluster-lensed SNe Ia (from the ground or space) to help illuminate the dark-matter distribution in clusters of galaxies, through the direct determination of absolute magnifications.
C1 [Patel, Brandon; McCully, Curtis; Jha, Saurabh W.; Holoien, Thomas W. -S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Rodney, Steven A.; Jones, David O.; Graur, O. R.; Riess, Adam G.; Ford, Holland; Lemze, Doron; Medezinski, Elinor; Zheng, Wei] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Graur, O. R.; Maoz, Dan] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Graur, O. R.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
[Graur, O. R.] NYU, CCPP 4, New York, NY 10003 USA.
[Merten, Julian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zitrin, Adi] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Riess, Adam G.; Koekemoer, Anton; Strolger, Louis G.] Space Telescope Sci Inst, Baltimore, MD 21208 USA.
[Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Sako, Masao] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Bartelmann, Matthias] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Balestra, Italo; Nonino, Mario] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy.
[Balestra, Italo] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy.
[Benitez, Narciso; Molino, Alberto] Inst Astrofis Andalucia CSIC, E-18008 Granada, Spain.
[Bouwens, Rychard] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Broadhurst, Tom] Univ Basque Country, Dept Theoret Phys, E-48080 Bilbao, Spain.
[Cenko, S. Bradley] NASA GSFC, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Cenko, S. Bradley; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Garnavich, Peter] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Grillo, Claudio] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Infante, Leopoldo] Pontificia Univ Catolica Chile, Inst Astrophys, Santiago, Chile.
[Jouvel, Stephanie] Inst Ciencias Espai IEEC CSIC, E-08913 Bellaterra, Barcelona, Spain.
[Kelson, Daniel] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Lahav, Ofer] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[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.
[Meneghetti, Massimo] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Meneghetti, Massimo] INFN, I-40127 Bologna, Italy.
[Meneghetti, Massimo] INFN, Sez Bologna, I-40127 Bologna, Italy.
[Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA.
[Rosati, Piero] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy.
[Rosati, Piero] ESO European So Observ, D-85748 Garching, Germany.
[Seitz, Stella] Univ Sternwarte, D-81679 Munich, Germany.
[Umetsu, Keiichi] Acad Sin, Inst Astron & Astrophys, Taipei 10617, Taiwan.
RP Patel, B (reprint author), Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
EM bpatel02@physics.rutgers.edu
RI Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015;
OI Grillo, Claudio/0000-0002-5926-7143; Meneghetti,
Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662;
Koekemoer, Anton/0000-0002-6610-2048; Benitez,
Narciso/0000-0002-0403-7455; Balestra, Italo/0000-0001-9660-894X; Graur,
Or/0000-0002-4391-6137; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas,
Leonidas/0000-0003-3030-2360
FU [GN-2012A-Q-32]; [GN-2013A-Q-25]
FX Additional data were obtained at the Gemini Observatory, which is
operated by the Association of Universities for Research in Astronomy,
Inc., under a cooperative agreement with the NSF on behalf of the Gemini
partnership: the National Science Foundation (United States), the
National Research Council (Canada), CONICYT (Chile), the Australian
Research Council (Australia), Ministerio da Ciencia, Tecnologia e
Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion
Productiva (Argentina). The data were taken as part of programs
GN-2012A-Q-32 and GN-2013A-Q-25.
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 MAY 1
PY 2014
VL 786
IS 1
AR 9
DI 10.1088/0004-637X/786/1/9
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH0LF
UT WOS:000335810700009
ER
PT J
AU Quintana, EV
Lissauer, JJ
AF Quintana, Elisa V.
Lissauer, Jack J.
TI THE EFFECT OF PLANETS BEYOND THE ICE LINE ON THE ACCRETION OF VOLATILES
BY HABITABLE-ZONE ROCKY PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; planets and satellites: composition; planets and
satellites: dynamical evolution and stability; planets and satellites:
formation; planets and satellites: terrestrial planets
ID HIGH-RESOLUTION SIMULATIONS; BINARY STAR SYSTEMS; EARTH-LIKE PLANETS;
TERRESTRIAL PLANETS; WATER DELIVERY; COLLISIONS; ASTEROIDS; RATIO;
TIMESCALES; DIVERSITY
AB Models of planet formation have shown that giant planets have a large impact on the number, masses, and orbits of terrestrial planets that form. In addition, they play an important role in delivering volatiles from material that formed exterior to the snow line (the region in the disk beyond which water ice can condense) to the inner region of the disk where terrestrial planets can maintain liquid water on their surfaces. We present simulations of the late stages of terrestrial planet formation from a disk of protoplanets around a solar-type star and we include a massive planet (from 1M(circle plus) to 1 M-J) in Jupiter's orbit at similar to 5.2 AU in all but one set of simulations. Two initial disk models are examined with the same mass distribution and total initial water content, but with different distributions of water content. We compare the accretion rates and final watermass fraction of the planets that form. Remarkably, all of the planets that formed in our simulations without giant planets were water-rich, showing that giant planet companions are not required to deliver volatiles to terrestrial planets in the habitable zone. In contrast, an outer planet at least several times the mass of Earth may be needed to clear distant regions of debris truncating the epoch of frequent large impacts. Observations of exoplanets from radial velocity surveys suggest that outer Jupiter-like planets may be scarce, therefore, the results presented here suggest that there may be more habitable planets residing in our galaxy than previously thought.
C1 [Quintana, Elisa V.] SETI Inst, Mountain View, CA 94043 USA.
[Quintana, Elisa V.; Lissauer, Jack J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div 245 3, Moffett Field, CA 94035 USA.
RP Quintana, EV (reprint author), SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA.
EM elisa.quintana@nasa.gov
FU NASA Ames Team of the NASA Astrobiology Institute
FX This work was funded in part by the NASA Ames Team of the NASA
Astrobiology Institute. E.V.Q. thanks Tom Barclay for useful discussions
and assistance with the figures.
NR 42
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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 MAY 1
PY 2014
VL 786
IS 1
AR 33
DI 10.1088/0004-637X/786/1/33
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH0LF
UT WOS:000335810700033
ER
PT J
AU Tang, SM
Bildsten, L
Wolf, WM
Li, KL
Kong, AKH
Cao, Y
Cenko, SB
De Cia, A
Kasliwal, MM
Kulkarni, SR
Laher, RR
Masci, F
Nugent, PE
Perley, DA
Prince, TA
Surace, J
AF Tang, Sumin
Bildsten, Lars
Wolf, William M.
Li, K. L.
Kong, Albert K. H.
Cao, Yi
Cenko, S. Bradley
De Cia, Annalisa
Kasliwal, Mansi M.
Kulkarni, Shrinivas R.
Laher, Russ R.
Masci, Frank
Nugent, Peter E.
Perley, Daniel A.
Prince, Thomas A.
Surace, Jason
TI AN ACCRETING WHITE DWARF NEAR THE CHANDRASEKHAR LIMIT IN THE ANDROMEDA
GALAXY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : individual (M31); novae, cataclysmic variables; supernovae :
general; white dwarfs; X-rays : binaries
ID REMARKABLE RECURRENT NOVA; STELLAR ASTROPHYSICS MESA; X-RAY SOURCES;
CLASSICAL NOVAE; PHOTOMETRIC CALIBRATION; CENTRAL REGION; LIGHT CURVES;
U SCORPII; TELESCOPE; M31
AB The intermediate Palomar Transient Factory (iPTF) detection of the most recent outburst of the recurrent nova (RN) system RX J0045.4+4154 in the Andromeda galaxy has enabled the unprecedented study of a massive (M > 1.3 M (circle dot)) accreting white dwarf (WD). We detected this nova as part of the near-daily iPTF monitoring of M31 to a depth of R approximate to 21 mag and triggered optical photometry, spectroscopy and soft X-ray monitoring of the outburst. Peaking at an absolute magnitude of M-R = -6.6 mag, and with a decay time of 1 mag per day, it is a faint and very fast nova. It shows optical emission lines of He/N and expansion velocities of 1900-2600 km s(-1) 1-4 days after the optical peak. The Swift monitoring of the X-ray evolution revealed a supersoft source (SSS) with kT(eff) approximate to 90-110 eV that appeared within 5 days after the optical peak, and lasted only 12 days. Most remarkably, this is not the first event from this system, rather it is an RN with a time between outbursts of approximately 1 yr, the shortest known. Recurrent X-ray emission from this binary was detected by ROSAT in 1992 and 1993, and the source was well characterized as a M > 1.3 M (circle dot) WD SSS. Based on the observed recurrence time between different outbursts, the duration and effective temperature of the SS phase, MESA models of accreting WDs allow us to constrain the accretion rate to M > 1.7 Chi 10(-7) M-circle dot yr(-1) and WD mass > 1.30 M-circle dot. If the WD keeps 30% of the accreted material, it will take less than a Myr to reach core densities high enough for carbon ignition (if made of C/O) or electron capture (if made of O/Ne) to end the binary evolution.
C1 [Tang, Sumin; Bildsten, Lars] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Tang, Sumin; Cao, Yi; Kulkarni, Shrinivas R.; Perley, Daniel A.; Prince, Thomas A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Bildsten, Lars; Wolf, William M.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Li, K. L.; Kong, Albert K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan.
[Li, K. L.; Kong, Albert K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan.
[Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[De Cia, Annalisa] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Kasliwal, Mansi M.] Carnegie Inst Washington Observ, Pasadena, CA 91101 USA.
[Laher, Russ R.; Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Masci, Frank] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Nugent, Peter E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Tang, SM (reprint author), Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
OI Wolf, William/0000-0002-6828-0630
FU National Science Foundation [PHY 11-25915, AST 11-09174, AST 12-05574];
Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231];
National Science Council of the Republic of China (Taiwan)
[NSC101-2119-M-008-007-MY3]; Hubble Fellowship; Carnegie-Princeton
Fellowship
FX This work was supported by the National Science Foundation under grants
PHY 11-25915, AST 11-09174, and AST 12-05574. Most of the MESA
simulations for this work were made possible by the Triton Resource. The
Triton Resource is a high-performance research computing system operated
by the San Diego Supercomputer Center at UC San Diego. 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 Contract No. DE-AC02-05CH11231. A.K.H.K. is
supported by the National Science Council of the Republic of China
(Taiwan) through grant NSC101-2119-M-008-007-MY3. M.M.K. acknowledges
generous support from the Hubble Fellowship and Carnegie-Princeton
Fellowship. We are grateful to the Swift Team for the superb timely
scheduling of the observations and providing data and analysis tools,
and to Bill Paxton for his development of MESA.
NR 59
TC 25
Z9 25
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2014
VL 786
IS 1
AR 61
DI 10.1088/0004-637X/786/1/61
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH0LF
UT WOS:000335810700061
ER
PT J
AU Wylezalek, D
Vernet, J
De Breuck, C
Stern, D
Brodwin, M
Galametz, A
Gonzalez, AH
Jarvis, M
Hatch, N
Seymour, N
Stanford, SA
AF Wylezalek, Dominika
Vernet, Joel
De Breuck, Carlos
Stern, Daniel
Brodwin, Mark
Galametz, Audrey
Gonzalez, Anthony H.
Jarvis, Matt
Hatch, Nina
Seymour, Nick
Stanford, Spencer A.
TI THE GALAXY CLUSTER MID-INFRARED LUMINOSITY FUNCTION AT 1.3 < z < 3.2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: clusters: general; galaxies: evolution;
galaxies: formation; galaxies: high-redshift; galaxies: luminosity
function, mass function; techniques: photometric
ID STELLAR POPULATION SYNTHESIS; COLOR-MAGNITUDE RELATION; REDSHIFT RADIO
GALAXIES; ACTIVE GALACTIC NUCLEI; SOUTH-POLE TELESCOPE; IRAC SHALLOW
SURVEY; H-ALPHA EMITTERS; STAR-FORMATION; FUNDAMENTAL-PLANE; HOST
GALAXIES
AB We present 4.5 mu m luminosity functions for galaxies identified in 178 candidate galaxy clusters at 1.3 < z < 3.2. The clusters were identified as Spitzer/Infrared Array Camera (IRAC) color-selected overdensities in the Clusters Around Radio-Loud AGN project, which imaged 420 powerful radio-loud active galactic nuclei (RLAGNs) at z > 1.3. The luminosity functions are derived for different redshift and richness bins, and the IRAC imaging reaches depths of m* + 2, allowing us to measure the faint end slopes of the luminosity functions. We find that alpha = -1 describes the luminosity function very well in all redshift bins and does not evolve significantly. This provides evidence that the rate at which the low mass galaxy population grows through star formation gets quenched and is replenished by in-falling field galaxies does not have a major net effect on the shape of the luminosity function. Our measurements for m* are consistent with passive evolution models and high formation redshifts (z(f) similar to 3). We find a slight trend toward fainter m* for the richest clusters, implying that the most massive clusters in our sample could contain older stellar populations, yet another example of cosmic downsizing. Modeling shows that a contribution of a star-forming population of up to 40% cannot be ruled out. This value, found from our targeted survey, is significantly lower than the values found for slightly lower redshift, z similar to 1, clusters found in wide-field surveys. The results are consistent with cosmic downsizing, as the clusters studied here were all found in the vicinity of RLAGNs-which have proven to be preferentially located in massive dark matter halos in the richest environments at high redshift-and they may therefore be older and more evolved systems than the general protocluster population.
C1 [Wylezalek, Dominika; Vernet, Joel; De Breuck, Carlos] European So Observ, D-85748 Garching, Germany.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Galametz, Audrey] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy.
[Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Jarvis, Matt] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Jarvis, Matt] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa.
[Hatch, Nina] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Seymour, Nick] CASS, Epping, NSW 1710, Australia.
[Stanford, Spencer A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, Spencer A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
RP Wylezalek, D (reprint author), European So Observ, Karl Schwarzschildstr 2, D-85748 Garching, Germany.
OI Hatch, Nina/0000-0001-5600-0534; Vernet, Joel/0000-0002-8639-8560;
Seymour, Nicholas/0000-0003-3506-5536; De Breuck,
Carlos/0000-0002-6637-3315
FU ARC Future Fellowship; NASA
FX We thank the referee for helpful comments that have improved the
manuscript. We gratefully thank Mark Lacy for allowing us to access
SERVS images and catalogs and Roberto Assef and Conor Mancone for
helpful discussions and advice. N. Seymour is the recipient of an ARC
Future Fellowship. 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.
NR 61
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 MAY 1
PY 2014
VL 786
IS 1
AR 17
DI 10.1088/0004-637X/786/1/17
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH0LF
UT WOS:000335810700017
ER
PT J
AU Turner, DD
Ferrare, RA
Wulfmeyer, V
Scarino, AJ
AF Turner, D. D.
Ferrare, R. A.
Wulfmeyer, V.
Scarino, A. J.
TI Aircraft Evaluation of Ground-Based Raman Lidar Water Vapor Turbulence
Profiles in Convective Mixed Layers
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
DE Boundary layer; Mass fluxes/transport; Water vapor; Lidars/Lidar
observations
ID SOUTHERN GREAT-PLAINS; ATMOSPHERIC BOUNDARY-LAYER; LARGE-EDDY
SIMULATION; AEROSOL EXTINCTION; DOPPLER LIDAR; VERTICAL VELOCITY;
RADAR-RASS; WRF MODEL; CLOUDS; STATISTICS
AB High temporal and vertical resolution water vapor measurements by Raman and differential absorption lidar systems have been used to characterize the turbulent fluctuations in the water vapor mixing ratio field in convective mixed layers. Since daytime Raman lidar measurements are inherently noisy (due to solar background and weak signal strengths), the analysis approach needs to quantify and remove the contribution of the instrument noise in order to derive the desired atmospheric water vapor mixing ratio variance and skewness profiles. This is done using the approach outlined by Lenschow et al.; however, an intercomparison with in situ observations was not performed. Water vapor measurements were made by a diode laser hygrometer flown on a Twin Otter aircraft during the Routine Atmospheric Radiation Measurement (ARM) Program Aerial Facility Clouds with Low Optical Water Depths Optical Radiative Observations (RACORO) field campaign over the ARM Southern Great Plains (SGP) site in 2009. Two days with Twin Otter flights were identified where the convective mixed layer was quasi stationary, and hence the 10-s, 75-m data from the SGP Raman lidar could be analyzed to provide profiles of water vapor mixing ratio variance and skewness. Airborne water vapor observations measured during level flight legs were compared to the Raman lidar data, demonstrating good agreement in both variance and skewness. The results also illustrate the challenges of comparing a point sensor making measurements over time to a moving platform making similar measurements horizontally.
C1 [Turner, D. D.] NOAA, Natl Severe Storms Lab, Norman, OK 73072 USA.
[Ferrare, R. A.] NASA Langley Res Ctr, Hampton, VA USA.
[Wulfmeyer, V.] Univ Hohenheim, Stuttgart, Germany.
[Scarino, A. J.] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Turner, DD (reprint author), NOAA, Natl Severe Storms Lab, 120 David L Boren Blvd, Norman, OK 73072 USA.
EM dave.turner@noaa.gov
FU NOAA's National Severe Storms Laboratory; Department of Energy (DOE)
Atmospheric System Research (ASR); NASA Science Mission Directorate; ASR
program [DE-AI02-05ER63985]; DOE Office of Science, Office of Biological
and Environmental Research (OBER); NASA CALIPSO project
FX NOAA's National Severe Storms Laboratory and the Department of Energy
(DOE) Atmospheric System Research (ASR) program supported this work. We
thank the Raman lidar mentor team of Chris Martin, John Goldsmith, and
Rob Newsom for their efforts in maintaining the Raman lidar. We would
also like to thank the entire RACORO team: Andy Vogelmann for his
leadership before, during, and after the experiment; the RACORO
scientific steering committee; Haf Jonsson for the analysis and
processing of the Twin Otter flight data; Glen Diskin for the DLH
processing; and the AAF for its coordination of the RACORO flight
activities. The data used in this paper were collected as part of ARM,
and are available via its online data archive
(http://www.archive.arm.gov). HSRL operations were supported by the NASA
Science Mission Directorate, the ASR program (Interagency Agreement
DE-AI02-05ER63985), the DOE Office of Science, Office of Biological and
Environmental Research (OBER), and the NASA CALIPSO project. The authors
thank the NASA Langley King Air B-200 flight crew for its outstanding
work supporting these flights and measurements. Finally, we thank Mike
Coniglio, Andy Vogelmann, Glenn Diskin, and Haf Jonsson for providing
comments on an earlier draft of this manuscript, and especially the two
anonymous reviewers for their excellent input, which improved this
manuscript.
NR 38
TC 11
Z9 11
U1 0
U2 17
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 MAY
PY 2014
VL 31
IS 5
BP 1078
EP 1088
DI 10.1175/JTECH-D-13-00075.1
PG 11
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA AH1LF
UT WOS:000335881600004
ER
PT J
AU Kwok, R
Markus, T
Morison, J
Palm, SP
Neumann, TA
Brunt, KM
Cook, WB
Hancock, DW
Cunningham, GF
AF Kwok, R.
Markus, T.
Morison, J.
Palm, S. P.
Neumann, T. A.
Brunt, K. M.
Cook, W. B.
Hancock, D. W.
Cunningham, G. F.
TI Profiling Sea Ice with a Multiple Altimeter Beam Experimental Lidar
(MABEL)
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
DE Remote sensing; Altimetry; Satellite observations; Sea ice; Lidars/Lidar
observations; Ice thickness
ID MISSION; SHEET
AB The sole instrument on the upcoming Ice, Cloud, and Land Elevation Satellite (ICESat-2) altimetry mission is a micropulse lidar that measures the time of flight of individual photons from laser pulses transmitted at 532 nm. Prior to launch, the Multiple Altimeter Beam Experimental Lidar (MABEL) serves as an airborne implementation for testing and development. This paper provides a first examination of MABEL data acquired on two flights over sea ice in April 2012: one north of the Arctic coast of Greenland and the other in the east Greenland Sea. The phenomenology of photon distributions in the sea ice returns is investigated. An approach to locate the surface and estimate its elevation in the distributions is described, and its achievable precision is assessed. Retrieved surface elevations over relatively flat leads in the ice cover suggest that precisions of several centimeters are attainable. Restricting the width of the elevation window used in the surface analysis can mitigate potential biases in the elevation estimates due to subsurface returns at 532 nm. Comparisons of nearly coincident elevation profiles from MABEL with those acquired by an analog lidar show good agreement. Discrimination of ice and open water, a crucial step in the determination of sea ice freeboard and the estimation of ice thickness, is facilitated by contrasts in the observed signal-background photon statistics. Future flight paths will sample a broader range of seasonal ice conditions for further evaluation of the year-round profiling capabilities and limitations of the MABEL instrument.
C1 [Kwok, R.; Cunningham, G. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Markus, T.; Neumann, T. A.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
[Morison, J.] Univ Washington, Polar Sci Ctr, Seattle, WA 98195 USA.
[Palm, S. P.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Brunt, K. M.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
[Brunt, K. M.] NASA, Goddard Space Flight Ctr, GESTAR, Greenbelt, MD 20771 USA.
[Cook, W. B.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Processes Lab, Greenbelt, MD 20771 USA.
[Hancock, D. W.] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ron.kwok@jpl.nasa.gov
RI Kwok, Ron/A-9762-2008; Neumann, Thomas/D-5264-2012
OI Kwok, Ron/0000-0003-4051-5896;
FU NASA's Airborne Science Program; National Aeronautics and Space
Administration
FX The digital camera system (DCS) on the ER-2 is operated and maintained
by the Airborne Sensor Facility under the auspices of NASA's Airborne
Science Program. RK and GFC carried out this work at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 14
TC 7
Z9 9
U1 3
U2 13
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 MAY
PY 2014
VL 31
IS 5
BP 1151
EP 1168
DI 10.1175/JTECH-D-13-00120.1
PG 18
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA AH1LF
UT WOS:000335881600009
ER
PT J
AU Schubert, SD
Wang, HL
Koster, RD
Suarez, MJ
Groisman, PY
AF Schubert, Siegfried D.
Wang, Hailan
Koster, Randal D.
Suarez, Max J.
Groisman, Pavel Ya.
TI Northern Eurasian Heat Waves and Droughts
SO JOURNAL OF CLIMATE
LA English
DT Review
DE Hydrologic cycle; Anticyclones; Waves, atmospheric; Climate variability;
Drought; Atmosphere-land interaction
ID SOIL-MOISTURE; ATMOSPHERIC BLOCKING; SURFACE-TEMPERATURE; CLIMATE
EXTREMES; EUROPEAN SUMMER; ANNULAR MODE; SEA-ICE; PRECIPITATION;
HEMISPHERE; TELECONNECTION
AB This article reviews the understanding of the characteristics and causes of northern Eurasian summertime heat waves and droughts. Additional insights into the nature of temperature and precipitation variability in Eurasia on monthly to decadal time scales and into the causes and predictability of the most extreme events are gained from the latest generation of reanalyses and from supplemental simulations with the NASA Goddard Earth Observing System model, version 5 (GEOS-5). Key new results are 1) the identification of the important role of summertime stationary Rossby waves in the development of the leading patterns of monthly Eurasian surface temperature and precipitation variability (including the development of extreme events such as the 2010 Russian heat wave); 2) an assessment of the mean temperature and precipitation changes that have occurred over northern Eurasia in the last three decades and their connections to decadal variability and global trends in SST; and 3) the quantification (via a case study) of the predictability of the most extreme simulated heat wave/drought events, with some focus on the role of soil moisture in the development and maintenance of such events. A literature survey indicates a general consensus that the future holds an enhanced probability of heat waves across northern Eurasia, while there is less agreement regarding future drought, reflecting a greater uncertainty in soil moisture and precipitation projections. Substantial uncertainties remain in the understanding of heat waves and drought, including the nature of the interactions between the short-term atmospheric variability associated with such extremes and the longer-term variability and trends associated with soil moisture feedbacks, SST anomalies, and an overall warming world.
C1 [Schubert, Siegfried D.; Wang, Hailan; Koster, Randal D.; Suarez, Max J.] NASA, GSFC, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Groisman, Pavel Ya.] Natl Climat Ctr, Asheville, NC USA.
RP Schubert, SD (reprint author), NASA, GSFC, Global Modeling & Assimilat Off, NASA GSFC Code 610-1, Greenbelt, MD 20771 USA.
EM siegfried.d.schubert@nasa.gov
RI Koster, Randal/F-5881-2012
OI Koster, Randal/0000-0001-6418-6383
FU NASA Modeling, Analysis, and Prediction (MAP) Program; NOAA/NASA
[NNX13AJ02G]; Ministry of Education and Science of the Russian
Federation [14.B25.31.0026]; WCRP; ESA-ESRIN; NASA; NIDIS; NSF; GEO;
USCLIVAR; NOAA
FX Support for this project was provided by the NASA Modeling, Analysis,
and Prediction (MAP) Program. Research of Pavel Groisman was supported
by NOAA/NASA (Grant NNX13AJ02G) and Grant 14.B25.31.0026 of the Ministry
of Education and Science of the Russian Federation. The lead author
would like to thank Anna Borovikov for helping to translate some of the
Russian language literature. We also wish to thank two anonymous
reviewers for their helpful comments and suggestions for improving the
manuscript. The NOAA GHCN gridded V2 data, the NOAA Merged Air Land and
SST Anomalies data, the NASA GPCP precipitation, and the NOAA PRECL
precipitation data were obtained from NOAA/OAR/ESRL PSD from their
website at http://www.esrl.noaa.gov/psd/. This paper is part of a
special collection devoted to our understanding of drought throughout
the world. The idea for this collection came about as a recommendation
of a 2012 international workshop on the development of a Global Drought
Information System (GDIS) sponsored by WCRP and various partner
organizations (ESA-ESRIN, NASA, NIDIS, NSF, GEO, USCLIVAR, and NOAA).
NR 134
TC 27
Z9 28
U1 6
U2 56
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 MAY
PY 2014
VL 27
IS 9
BP 3169
EP 3207
DI 10.1175/JCLI-D-13-00360.1
PG 39
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AG9EI
UT WOS:000335721800002
ER
PT J
AU Som, SM
AF Som, Sanjoy M.
TI PLANETARY SCIENCE Into thin martian air
SO NATURE GEOSCIENCE
LA English
DT News Item
ID EARLY MARS; CLIMATE
AB A dense early atmosphere has been invoked to explain the strong greenhouse effect inferred for early Mars. Yet an analysis of the smallest impact craters suggests that the atmospheric pressure on Mars 3.6 billion years ago was surprisingly low.
C1 [Som, Sanjoy M.] NASA, Ames Res Ctr, Blue Marble Space Inst Sci, Exobiol Branch, Moffett Field, CA 94035 USA.
[Som, Sanjoy M.] NASA, Ames Res Ctr, Flight Syst Implementat Branch, Moffett Field, CA 94035 USA.
RP Som, SM (reprint author), NASA, Ames Res Ctr, Blue Marble Space Inst Sci, Exobiol Branch, Moffett Field, CA 94035 USA.
EM sanjoy@bmsis.org
NR 11
TC 0
Z9 0
U1 1
U2 12
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD MAY
PY 2014
VL 7
IS 5
BP 329
EP 330
DI 10.1038/ngeo2145
PG 2
WC Geosciences, Multidisciplinary
SC Geology
GA AH2JZ
UT WOS:000335948600005
ER
PT J
AU Neu, JL
Flury, T
Manney, GL
Santee, ML
Livesey, NJ
Worden, J
AF Neu, Jessica L.
Flury, Thomas
Manney, Gloria L.
Santee, Michelle L.
Livesey, Nathaniel J.
Worden, John
TI Tropospheric ozone variations governed by changes in stratospheric
circulation
SO NATURE GEOSCIENCE
LA English
DT Article
ID QUASI-BIENNIAL OSCILLATION; TRENDS; MODEL; VARIABILITY; CHEMISTRY;
EXCHANGE; ENSO
AB The downward transport of stratospheric ozone is an important natural source of tropospheric ozone, particularly in the upper troposphere, where changes in ozone have their largest radiative effect(1). Stratospheric circulation is projected to intensify over the coming century, which could lead to an increase in the flux of ozone from the stratosphere to the troposphere(2-4). However, large uncertainties in the stratospheric contribution to trends and variability in tropospheric ozone levels(5-7) make it difficult to reliably project future changes in tropospheric ozone(8). Here, we use satellite measurements of stratospheric water vapour and tropospheric ozone levels collected between 2005 and 2010 to assess the effect of changes in stratospheric circulation, driven by El Nino/Southern Oscillation and the stratospheric Quasi-Biennial Oscillation, on tropospheric ozone levels. Wefindthat interannual variations in the strength of the stratospheric circulation of around 40%-comparable to the mean change in stratospheric circulation projected this century(2)-lead to changes in tropospheric ozone levels in the northern mid-latitudes of around 2%, approximately half of the interannual variability. Assuming that the observed response of tropospheric ozone levels to interannual variations in circulation is a good predictor of its equilibrium response, we suggest that the projected intensification of the stratospheric circulation over the coming century could lead to small but important increases in tropospheric ozone levels.
C1 [Neu, Jessica L.; Flury, Thomas; Santee, Michelle L.; Livesey, Nathaniel J.; Worden, John] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Manney, Gloria L.] NorthWest Res Associates, Socorro, NM 87801 USA.
[Manney, Gloria L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA.
RP Neu, JL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jessica.l.neu@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX We thank the MLS and TES science teams and the Aura project for their
support. We also thank J-F. Lamarque and D. Kinnison of the National
Center for Atmospheric Research for providing CAM-Chem and WACCM
modelling results, respectively, H. Nguyen of the Jet Propulsion
Laboratory for help with the statistical analysis, T. Shepherd of the
University of Reading for allowing us to include results from the CMAM
model, and S. Hardiman of the UK Meterological Office for providing
model residual vertical velocities. 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 30
TC 31
Z9 31
U1 1
U2 37
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD MAY
PY 2014
VL 7
IS 5
BP 340
EP 344
DI 10.1038/ngeo2138
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA AH2JZ
UT WOS:000335948600010
ER
PT J
AU Xu, HF
Shen, ZZ
Konishi, H
Fu, PQ
Szlufarska, I
AF Xu, Huifang
Shen, Zhizhang
Konishi, Hiromi
Fu, Pingqiu
Szlufarska, Izabela
TI Crystal structures of laihunite and intermediate phases between
laihunite-1M and fayalite: Z-contrast imaging and ab initio study
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Laihunite; vacancy ordering; Z-contrast imaging; DFT; HRTEM;
superstructure; olivine; oxidation
ID OLIVINE; OXIDATION; MICROSCOPY; SERPENTINE
AB Crystals of laihunite from Xiaolaihe of Liaoning Province, northeast China, were studied using selected-area electron diffraction (SAED), high-resolution transmission electron microscopy (HRTEM), and Z-contrast imaging. Z-contrast images directly reveal ordered vacancies in M1 sites. The results confirm early structural models for 1-layer laihunite (or laihunite-1M) with ideal stoichiometry of square 0 5Fe0.52+Fe3+SiO4. 2-layer laihunite and 3-layer laihunite are found to be chemically different from laihunite-1M. The 2-layer laihunite can be viewed as a periodic intergrowth of laihunite and fayalite in the 1:1 ratio. The 3-layer laihunite can be considered to be a periodic intergrowth of laihunite and fayalite in the 1:0.5 ratio along the c-axis. Ideal stoichiometries for the 2-layer structure and the 3-layer structure are square 0.5Fe2.52+Fe3+[SiO4](2) and square 1.0Fe3.02+Fe2.03+[SiO4](3), respectively. The structural intergrowth of the 3-layer laihunite and the 1-layer lahunite results in chemical compositions falling within the range between the two aforementioned structures, such as the chemical formula of square 0.4Fe0.82+Fe0.83+SiO4, reported earlier in the literature.
The crystal structures of the 1-layer laihunite (1M), the 2-layer laihunite (2M), and the 3-layer laihunite (3Or) determined from Z-contrast images and ab initio calculations using the density functional theory (DFT) have space groups of P2(1)/b, P2(1)/b, and Pbnm, respectively. The previously reported monoclinic symmetry for the 3-layer laihunite may be an artifact due to overlapping diffraction spots from both, the laihunite-3 Or and the laihunite-1M. Our study demonstrates that the method of combining Z-contrast imaging and ab initio calculation can be effectively used for identifying structures of nano-phases in host crystals. Perhaps more importantly, Z-contrast imaging provides a powerful means for direct observation of vacancies and other defects, and may be utilized to map vacancies in Fe3+-bearing olivines, the alignments of which can greatly affect anisotropic diffusion in such structures.
C1 [Xu, Huifang; Shen, Zhizhang; Konishi, Hiromi] Univ Wisconsin, NASA Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA.
[Fu, Pingqiu] Chinese Acad Sci, Inst Geochem, Guiyang 550002, Guizhou, Peoples R China.
[Szlufarska, Izabela] Univ Wisconsin, Dept Mat Sci & Engn, Madison, WI 53706 USA.
RP Xu, HF (reprint author), Univ Wisconsin, NASA Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA.
EM hfxu@geology.wisc.edu
FU NASA Astrobiology Institute [N07-5489]; NSF [EAR-095800]; Major Research
Instrumentation (MRI) program of NSF; K. C. Wong Education Foundation
(Hong Kong)
FX This work is supported by NASA Astrobiology Institute (N07-5489) and NSF
(EAR-095800). Authors thank Alex Kivit for optimizing instrument
condition. Author also thank Major Research Instrumentation (MRI)
program of NSF for funding the aberration corretced STEM. Xu thanks
David Veblen for supporting his early TEM works at Johns Hopkins
University. Xu and Fu acknowledge K. C. Wong Education Foundation (Hong
Kong) for supporting early stage of this collaborative research.
NR 34
TC 7
Z9 7
U1 1
U2 14
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD MAY-JUN
PY 2014
VL 99
IS 5-6
BP 881
EP 889
DI 10.2138/am.2014.4691
PG 9
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA AG7YE
UT WOS:000335633900003
ER
PT J
AU Dyar, MD
Jawin, ER
Breves, E
Marchand, G
Nelms, M
Lane, MD
Mertzman, SA
Bish, DL
Bishop, JL
AF Dyar, M. Darby
Jawin, Erica R.
Breves, Elly
Marchand, Gerard
Nelms, Melissa
Lane, Melissa D.
Mertzman, Stanley A.
Bish, David L.
Bishop, Janice L.
TI Mossbauer parameters of iron in phosphate minerals: Implications for
interpretation of martian data
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Mossbauer; Mars; phosphates; alluaudite; arrojadite; vivianite;
triphylite
ID SOLID-SOLUTION SERIES; X-RAY SPECTROMETER; QUADRUPOLE SPLITTING
DISTRIBUTIONS; CRYSTAL-STRUCTURE DETERMINATION; TRIPLITE-TRIPLOIDITE
GROUP; ALLUAUDITE STRUCTURE TYPE; SAPUCAIA-PEGMATITE MINE;
MERIDIANI-PLANUM; SNC METEORITES; SYNTHETIC LIPSCOMBITE
AB Phosphate minerals, while relatively rare, show a broad range of crystal structure types with linkages among PO4 tetrahedra mimicking the hierarchy of polymerization of SiO4 tetrahedra seen in silicate minerals. To augment previous Mossbauer studies of individual phosphate species and groups of species, this paper presents new Mossbauer data on 63 different phosphate samples, and integrates them with data on more than 37 phosphate species in 62 other studies from the literature. Variations in Mossbauer parameters of different sites in each mineral are then related to both the local polyhedral environment around the Fe cations and the overall structural characteristics of each species. The entire aggregated Mossbauer data set on phosphate minerals is juxtaposed against parameters obtained for spectra from the MIMOS spectrometers on Mars. This comparison demonstrates that signatures from many different phosphate or sulfate mineral species could also be contributing to Mars Mossbauer spectra. Results underscore the conclusion that unique mineral identifications are generally not possible from Mossbauer data alone, particularly for paramagnetic phases, although combining Mossbauer results with other data sets enables a greater level of confidence in constraining mineralogy. This study provides a wealth of new data on Fe-bearing phosphate minerals to bolster future analyses of Mossbauer spectra acquired on Mars.
C1 [Dyar, M. Darby; Jawin, Erica R.; Breves, Elly; Marchand, Gerard; Nelms, Melissa] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
[Lane, Melissa D.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Mertzman, Stanley A.] Franklin & Marshall Coll, Dept Earth & Environm, Lancaster, PA 17603 USA.
[Bish, David L.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
[Bishop, Janice L.] NASA, SETI Inst, Ames Res Ctr, Mountain View, CA 94043 USA.
RP Dyar, MD (reprint author), Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
EM mdyar@mtholyoke.edu
FU NASA [NNX08AP42G]; NSF [MRI-0923224]
FX We are grateful to Ed Cloutis, the Harvard Mineralogical Museum, and the
NMNH for the loan of samples, and for support from NASA Grant
NNX08AP42G. Student support for this project was provided by the
Massachusetts Space Grant Consortium. We thank David Palmer for help
with the CrystalMaker models. Mertzman salutes the NSF for award
MRI-0923224, which enabled the purchase of PANalytical XRD system X'Pert
PRO equipped with a 15 position sample changer used in this study. This
is PSI Contribution Number 608.
NR 257
TC 8
Z9 8
U1 5
U2 28
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD MAY-JUN
PY 2014
VL 99
IS 5-6
BP 914
EP 942
DI 10.2138/am.2014.4701
PG 29
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA AG7YE
UT WOS:000335633900007
ER
PT J
AU McCollom, TM
Ehlmann, BL
Wang, A
Hynek, BM
Moskowitz, B
Berquo, TS
AF McCollom, Thomas M.
Ehlmann, Bethany L.
Wang, Alian
Hynek, Brian M.
Moskowitz, Bruce
Berquo, Thelma S.
TI Detection of iron substitution in natroalunite-natrojarosite solid
solutions and potential implications for Mars
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Mars; alunite group; visible/near infrared spectra; Raman spectra;
hydrothermal; acid-sulfate alteration
ID ACID-SULFATE ALTERATION; JAROSITE-GROUP; RAMAN-SPECTROSCOPY;
CRYSTAL-CHEMISTRY; MERIDIANI-PLANUM; ALUNITE; MOSSBAUER; SPECTROMETER;
MINERALS; HEMATITE
AB Natroalunite containing substantial amounts of Fe occurs as a prominent secondary phase during acid-sulfate alteration of pyroclastic basalts in volcanic fumaroles in Nicaragua and elsewhere, and has been observed in laboratory simulations of acid-sulfate alteration as well. Reaction path models constrained by field and experimental observations predict that Fe-rich natroalunite should also form as a major secondary phase during alteration of martian basalt under similar circumstances. Here, we evaluate the potential to use spectroscopic methods to identify minerals from the alunite group with chemical compositions intermediate between natroalunite and natrojarosite on the surface of Mars, and to remotely infer their Fe contents. X-ray diffraction and spectroscopic measurements (Raman, visible/near infrared, mid-infrared, Mossbauer) were obtained for a suite of synthetic solid solutions with a range of Fe contents ranging from natroalunite to natrojarosite. In the visible/near infrared, minerals with intermediate compositions display several spectral features not evident in end-member spectra that could be used to remotely identify these minerals and infer their composition. In addition, Raman spectra, mid-infrared spectra, and X-ray diffraction peaks all show systematic variation with changing Fe content, indicating that these methods could potentially be used to infer mineral compositions as well. The results suggest that alunite group minerals with intermediate Fe compositions may be able to account for some visible/near-infrared and Mossbauer spectral features from Mars that had previously been unidentified or attributed to other phases. Overall, our findings indicate that consideration of solid solutions may lead to new identifications of alunite group minerals on the surface of Mars, and raise the possibility that minerals with compositions intermediate between natroalunite and natrojarosite may be widely distributed on the planet.
C1 [McCollom, Thomas M.; Hynek, Brian M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Hynek, Brian M.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
[Ehlmann, Bethany L.] CALTECH, Pasadena, CA 91125 USA.
[Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wang, Alian] Washington Univ, Deptartment Earth & Planetary Sci, St Louis, MO 63130 USA.
[Wang, Alian] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
[Moskowitz, Bruce] Univ Minnesota, Dept Earth Sci, Minneapolis, MN 55455 USA.
[Moskowitz, Bruce] Univ Minnesota, Inst Rock Magnetism, Minneapolis, MN 55455 USA.
[Berquo, Thelma S.] Concordia Coll, Dept Phys, Moorhead, MN 56562 USA.
RP McCollom, TM (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
EM mccollom@lasp.colorado.edu
RI Berquo, Thelma/D-6359-2013
FU NASA Mars Fundamental Research Program [NNX12AI02G, NNX10AM89G]; NASA
Exobiology Award [NNX08AQ11G]; NASA Early Career Award [NNX12AF20G];
Instruments and Facilities Program, Division of Earth Science, National
Science Foundation
FX This research was supported by funds from NASA Mars Fundamental Research
Program grants NNX12AI02G (T.M.M.) and NNX10AM89G (A.W.), NASA
Exobiology Award NNX08AQ11G (T.M.M. and B.M.H.), and NASA Early Career
Award NNX12AF20G (B.M.H.). Thanks to George Rossman for assistance and
use of his FTIR spectrometer and to Frieder Klein for help with the
Raman analysis of natural samples. The authors are grateful for reviews
by Gregg Swayze and Stuart Mills, whose thoughtful comments helped to
improve the manuscript. The Institute for Rock Magnetism is supported by
grants from the Instruments and Facilities Program, Division of Earth
Science, National Science Foundation.
NR 53
TC 15
Z9 15
U1 3
U2 20
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD MAY-JUN
PY 2014
VL 99
IS 5-6
BP 948
EP 964
DI 10.2138/am.2014.4617
PG 17
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA AG7YE
UT WOS:000335633900009
ER
PT J
AU Papike, JJ
Burger, PV
Bell, AS
Shearer, CK
Le, LA
Jones, J
Provencio, P
AF Papike, James J.
Burger, Paul V.
Bell, Aaron S.
Shearer, Charles K.
Le, Loan
Jones, John
Provencio, Paula
TI Valence state partitioning of V between pyroxene and melt for martian
melt compositions Y 980459 and QUE 94201: The effect of pyroxene
composition and crystal structure
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Vanadium; partitioning; pyroxene; orthopyroxene; augite; pigeonite;
EBSD; valence
ID OXYGEN FUGACITY; UPPER-MANTLE; OLIVINE; BASALTS; MARS; PETROGENESIS;
CONSTRAINTS; SILICATES; VANADIUM; SPINEL
AB A martian basalt (Yamato 980459) composition was used to synthesize olivine, spinel, and pyroxene at 1200 degrees C at five oxygen fugacities: IW-1, IW, IW+1, IW+2, and QFM. The goal of this study is to examine the significant variation in the value of D-V(pyroxene/melt) with changing Wo content in pyroxene. While most literature on this subject relies on electron microprobe data that assumes that if the Wo component (CaSiO3) is <4 mol%, the pyroxene is in fact orthopyroxene, we've made a more robust identification of orthopyroxene using appropriate Kikuchi diffraction lines collected during electron backscatter diffraction analysis. We compare augite (Wo similar to 33), pigeonite (Wo similar to 13), orthopyroxene (Wo <4), and olivine. In augite (Wo similar to 33), the M2 site is 8-coordinated, while in pigeonite (Wo similar to 13), the site is 6-coordinated. The larger (8-coordinated) M2 site in augite requires structural expansion along the chain direction. The longer chain is enabled by the substitution of the larger Al for Si. The Al3+ substitution for Si4+ causes a charge deficiency that is made up, in part, by the substitution of V4+ and V3+ in the pyroxene M1 site. This rationale does not fully explain the dramatic decrease in D-V(orthopyroxene/melt). In monoclinic pyroxenes, the TOT stacking is characterized by + + + + (indicating the direction), a stacking pattern that produces a monoclinic offset. In orthopyroxene, the stacking is + + - -, which produces an orthorhombic structure. The M2 site is located between the reversed TOT units and is highly constrained to 6-coordination and thus cannot contain significant Ca that requires 8-coordination. Because the M2 site in orthopyroxene is small and constrained, it accommodates less Al in the tetrahedral chains and thus less V in the pyroxene M1 site.
C1 [Papike, James J.; Burger, Paul V.; Bell, Aaron S.; Shearer, Charles K.; Provencio, Paula] Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Le, Loan] NASA Johnson Space Ctr, JSC Engn Technol & Sci JETS, Houston, TX 77058 USA.
[Jones, John] NASA Johnson Space Ctr, Houston, TX 77058 USA.
RP Papike, JJ (reprint author), Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
EM pvburger@unm.edu
FU NASA Cosmochemistry program
FX We acknowledge support for this research from the NASA Cosmochemistry
program to Charles Shearer and John Jones.
NR 19
TC 2
Z9 3
U1 0
U2 6
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD MAY-JUN
PY 2014
VL 99
IS 5-6
BP 1175
EP 1178
DI 10.2138/am.2014.4788
PG 4
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA AG7YE
UT WOS:000335633900030
ER
PT J
AU Boening, C
AF Boening, Carmen
TI Detecting sea-level rise
SO NATURE CLIMATE CHANGE
LA English
DT Editorial Material
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91104 USA.
RP Boening, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91104 USA.
EM carmen.boening@jpl.nasa.gov
NR 8
TC 0
Z9 0
U1 2
U2 9
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 MAY
PY 2014
VL 4
IS 5
BP 327
EP 328
PG 2
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AG4PV
UT WOS:000335403500014
ER
PT J
AU Wang, Y
Lee, KH
Lin, Y
Levy, M
Zhang, RY
AF Wang, Yuan
Lee, Keun-Hee
Lin, Yun
Levy, Misti
Zhang, Renyi
TI Distinct effects of anthropogenic aerosols on tropical cyclones
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID HURRICANES; ATLANTIC; INTENSITY; IMPACTS; MODEL
AB Long-term observations have revealed large amplitude fluctuations in the frequency and intensity of tropical cyclones (TCs; refs 1-4), but the anthropogenic impacts, including greenhouse gases and particulate matter pollution(4,5), remain to be elucidated. Here, we show distinct aerosol effects on the development of TCs: the coupled microphysical and radiative effects of anthropogenic aerosols result in delayed development, weakened intensity and early dissipation, but an enlarged rainband and increased precipitation under polluted conditions. Our results imply that anthropogenic aerosols probably exhibit an opposite effect to that of greenhouse gases, highlighting the necessity of incorporating a realistic microphysical-radiative interaction of aerosols for accurate forecasting and climatic prediction of TCs in atmospheric models.
C1 [Wang, Yuan; Lee, Keun-Hee; Lin, Yun; Levy, Misti; Zhang, Renyi] Texas A&M Univ, Dept Atmospher Sci, Ctr Atmospher Chem & Environm, College Stn, TX 77843 USA.
[Wang, Yuan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lee, Keun-Hee] Korean Meteorol Adm, Seoul 156720, South Korea.
[Zhang, Renyi] Peking Univ, Coll Environm Sci & Engn, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100871, Peoples R China.
RP Wang, Y (reprint author), Texas A&M Univ, Dept Atmospher Sci, Ctr Atmospher Chem & Environm, College Stn, TX 77843 USA.
EM Yuan.Wang@jpl.nasa.gov; renyi-zhang@geos.tamu.edu
RI Levy, Misti/G-8660-2014; Lin, Yun/B-1906-2013; Zhang, Renyi/A-2942-2011;
OI Levy, Misti/0000-0002-4832-7753; Lin, Yun/0000-0001-8222-0346
FU NASA; Ministry of Science and Technology of China [2013CB955800]
FX Y.W. was supported by a NASA graduate fellowship in Earth Sciences. R.Z.
acknowledges support from the Ministry of Science and Technology of
China under award number 2013CB955800. We thank K.. Emanuel, P. Liss, C.
Schumacher and F. Zhang for helpful discussions. Supercomputing
computational facilities were provided by the Texas A&M University. Y.W.
acknowledges additional support by the NASA ROSES COUND program at the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA.
NR 33
TC 17
Z9 17
U1 4
U2 36
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 MAY
PY 2014
VL 4
IS 5
BP 368
EP 373
DI 10.1038/NCLIMATE2144
PG 6
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AG4PV
UT WOS:000335403500025
ER
PT J
AU Keppenne, CL
AF Keppenne, Christian L.
TI An ensemble recentering Kalman filter with an application to Argo
temperature data assimilation into the NASA GEOS-5 coupled model
SO OCEAN MODELLING
LA English
DT Article
DE Data assimilation; Kalman filter; Ensemble Kalman filter; Particle
filter; Coupled data assimilation
ID QUASI-GEOSTROPHIC MODEL; ALTIMETER DATA
AB A two-step ensemble recentering Kalman filter (ERKF) analysis scheme is introduced. The algorithm consists of a recentering step followed by an ensemble Kalman filter (EnKF) analysis step. The recentering step is formulated such as to adjust the prior distribution of an ensemble of model states so that the deviations of individual samples from the sample mean are unchanged but the original sample mean is shifted to the prior position of the most likely particle, where the likelihood of each particle is measured in terms of closeness to the assimilated observations. The computational cost of the ERKF is essentially the same as that of a same size EnKF.
The ERKF is applied to the assimilation of Argo temperature profiles into the OGCM component of an ensemble of NASA GEOS-5 coupled models. Unassimilated Argo salt data are used for validation. These data serve as a proxy to assess the potential of the ERKF to improve estimates of unobserved model variables. A surprisingly small number (16) of model trajectories is sufficient to significantly improve model estimates of salinity over estimates from an ensemble run without assimilation. The two-step algorithm also performs better than the EnKF although its performance is degraded in poorly observed regions. The efficacy of the recentering is attributed to its ability to preserve balance relationships between observed and unobserved variables, even when the ensemble size is too small for the EnKF to accurately estimate cross-field error covariances. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Keppenne, Christian L.] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Keppenne, Christian L.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Keppenne, CL (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM christian.keppenne@nasa.gov
FU NASA's Modeling Analysis and Prediction Program [WBS 802678.02.17.01.25]
FX This work is supported by NASA's Modeling Analysis and Prediction
Program under WBS 802678.02.17.01.25. The infrastructure for the runs is
provided by the NASA Center for Climate Simulation (NCCS). Yuri
Vikhliaev, Max Suarez and Bin Zhao helped configure the GEOS-5 modeling
system. Guillaume Vernieres helped configure the data assimilation
system and Robin Kovach assisted with the observation preprocessing and
with plotting the results. Eugenia Kalnay, Michele Rienecker and two
insightful anonymous reviewers helped interpreting the results and
improve the initial draft manuscript.
NR 14
TC 2
Z9 2
U1 0
U2 6
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1463-5003
EI 1463-5011
J9 OCEAN MODEL
JI Ocean Model.
PD MAY
PY 2014
VL 77
BP 50
EP 55
DI 10.1016/j.ocemod.2014.03.001
PG 6
WC Meteorology & Atmospheric Sciences; Oceanography
SC Meteorology & Atmospheric Sciences; Oceanography
GA AG9MT
UT WOS:000335744100004
ER
PT J
AU Mishchenko, MI
Liu, L
Cairns, B
Mackowski, DW
AF Mishchenko, Michael I.
Liu, Li
Cairns, Brian
Mackowski, Daniel W.
TI Optics of water cloud droplets mixed with black-carbon aerosols
SO OPTICS LETTERS
LA English
DT Article
ID T-MATRIX; SOLAR-RADIATION; SCATTERING; ABSORPTION; INCLUSIONS; PARTICLES
AB We use the recently extended superposition T-matrix method to calculate scattering and absorption properties of micrometer-sized water droplets contaminated by black carbon. Our numerically exact results reveal that, depending on the mode of soot-water mixing, the soot specific absorption can vary by a factor exceeding 6.5. The specific absorption is maximized when the soot material is quasi-uniformly distributed throughout the droplet interior in the form of numerous small monomers. The range of mixing scenarios captured by our computations implies a wide range of remote sensing and radiation budget implications of the presence of black carbon in liquid-water clouds. We show that the popular Maxwell-Garnett effective-medium approximation can be used to calculate the optical cross sections, single-scattering albedo, and asymmetry parameter for the quasi-uniform mixing scenario, but is likely to fail in application to other mixing scenarios and in computations of the elements of the scattering matrix. (C) 2014 Optical Society of America
C1 [Mishchenko, Michael I.; Liu, Li; Cairns, Brian] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Liu, Li] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[Mackowski, Daniel W.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 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; Mackowski, Daniel/K-1917-2013;
OI Cairns, Brian/0000-0002-1980-1022
NR 21
TC 17
Z9 17
U1 4
U2 19
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 MAY 1
PY 2014
VL 39
IS 9
BP 2607
EP 2610
DI 10.1364/OL.39.002607
PG 4
WC Optics
SC Optics
GA AG5YX
UT WOS:000335496400020
PM 24784057
ER
PT J
AU Aartsen, MG
Abbasi, R
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Altmann, D
Arguelles, C
Arlen, TC
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Baum, V
Bay, R
Beatty, JJ
Tjus, JB
Becker, KH
BenZvi, S
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Besson, DZ
Binder, G
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Bose, D
Boser, S
Botner, O
Brayeur, L
Bretz, HP
Brown, AM
Bruijn, R
Casey, J
Casier, M
Chirkin, D
Christov, A
Christy, B
Clark, K
Classen, L
Clevermann, F
Coenders, S
Cohen, S
Cowen, DF
Silva, AHC
Danninger, M
Daughhetee, J
Davis, JC
Day, M
de Andre, JPAM
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
Eichmann, B
Eisch, J
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
Gretskov, P
Groh, JC
Gross, A
Ha, C
Ismail, AH
Hallen, P
Hallgren, A
Halzen, F
Hanson, K
Hebecker, D
Heereman, D
Heinen, D
Helbing, K
Hellauer, R
Hickford, S
Hill, GC
Hoffman, KD
Hoffmann, R
Homeier, A
Hoshina, K
Huang, F
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
Kauer, M
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
Kriesten, A
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
Macias, 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
Palczewski, T
Paul, L
Pepper, JA
de los Heros, CP
Pfendner, C
Pieloth, D
Pinat, E
Posselt, J
Price, PB
Przybylski, GT
Quinnan, M
Radel, L
Rameez, M
Rawlins, K
Redl, P
Reimann, R
Resconi, E
Rhode, W
Ribordy, M
Richman, M
Riedel, B
Robertson, S
Rodrigues, JP
Rott, C
Ruhe, T
Ruzybayev, B
Ryckbosch, D
Saba, SM
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
Stanisha, NA
Stasik, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strahler, EA
Strom, R
Strotjohann, NL
Sullivan, GW
Taavola, H
Taboada, I
Tamburro, A
Tepe, A
Ter-Antonyan, S
Tesic, G
Tilav, S
Toale, PA
Tobin, MN
Toscano, S
Tselengidou, M
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
Whelan, B
Whitehorn, N
Wiebe, K
Wiebusch, CH
Williams, DR
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, DL
Xu, XW
Yanez, JP
Yodh, G
Yoshida, S
Zarzhitsky, P
Ziemann, J
Zierke, S
Zoll, M
AF Aartsen, M. G.
Abbasi, R.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Altmann, D.
Arguelles, C.
Arlen, T. C.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Baum, V.
Bay, R.
Beatty, J. J.
Tjus, J. Becker
Becker, K. -H.
BenZvi, S.
Berghaus, P.
Berley, D.
Bernardini, E.
Bernhard, A.
Besson, D. Z.
Binder, G.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Brayeur, L.
Bretz, H. -P.
Brown, A. M.
Bruijn, R.
Casey, J.
Casier, M.
Chirkin, D.
Christov, A.
Christy, B.
Clark, K.
Classen, L.
Clevermann, F.
Coenders, S.
Cohen, S.
Cowen, D. F.
Silva, A. H. Cruz
Danninger, M.
Daughhetee, J.
Davis, J. C.
Day, M.
de Andre, J. P. A. M.
De Clercq, C.
De Ridder, S.
Desiati, P.
de Vries, K. D.
de With, M.
DeYoung, T.
Diaz-Velez, J. C.
Dunkman, M.
Eagan, R.
Eberhardt, B.
Eichmann, B.
Eisch, J.
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.
Gretskov, P.
Groh, J. C.
Gross, A.
Ha, C.
Ismail, A. Haj
Hallen, P.
Hallgren, A.
Halzen, F.
Hanson, K.
Hebecker, D.
Heereman, D.
Heinen, D.
Helbing, K.
Hellauer, R.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Homeier, A.
Hoshina, K.
Huang, F.
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.
Kauer, M.
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.
Kriesten, A.
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.
Macias, 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.
Palczewski, T.
Paul, L.
Pepper, J. A.
Perez de los Heros, C.
Pfendner, C.
Pieloth, D.
Pinat, E.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Quinnan, M.
Raedel, L.
Rameez, M.
Rawlins, K.
Redl, P.
Reimann, R.
Resconi, E.
Rhode, W.
Ribordy, M.
Richman, M.
Riedel, B.
Robertson, S.
Rodrigues, J. P.
Rott, C.
Ruhe, T.
Ruzybayev, B.
Ryckbosch, D.
Saba, S. M.
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.
Stanisha, N. A.
Stasik, A.
Stezelberger, T.
Stokstad, R. G.
Stossl, A.
Strahler, E. A.
Strom, R.
Strotjohann, N. L.
Sullivan, G. W.
Taavola, H.
Taboada, I.
Tamburro, A.
Tepe, A.
Ter-Antonyan, S.
Tesic, G.
Tilav, S.
Toale, P. A.
Tobin, M. N.
Toscano, S.
Tselengidou, M.
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.
Whelan, B.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
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 Search for neutrino-induced particle showers with IceCube-40
SO PHYSICAL REVIEW D
LA English
DT Article
ID SCATTERING; SELECTION; CASCADES; SPECTRUM; AMANDA; SYSTEM; MODEL; ICE
AB We report on the search for neutrino-induced particle showers, so-called cascades, in the IceCube-40 detector. The data for this search were collected between April 2008 and May 2009 when the first 40 IceCube strings were deployed and operational. Three complementary searches were performed, each optimized for different energy regimes. The analysis with the lowest energy threshold (2 TeV) targeted atmospheric neutrinos. A total of 67 events were found, consistent with the expectation of 41 atmospheric muons and 30 atmospheric neutrino events. The two other analyses targeted a harder, astrophysical neutrino flux. The analysis with an intermediate threshold of 25 TeV leads to the observation of 14 cascadelike events, again consistent with the prediction of 3.0 atmospheric neutrino and 7.7 atmospheric muon events. We hence set an upper limit of E-2 Phi(lim) <= 7.46 x 10(-8) GeV sr(-1) s(-1) cm(-2) (90% C.L.) on the diffuse flux from astrophysical neutrinos of all neutrino flavors, applicable to the energy range 25 TeV to 5 PeV, assuming an E-nu(-2) spectrum and a neutrino flavor ratio of 1: 1: 1 at the Earth. The third analysis utilized a larger and optimized sample of atmospheric muon background simulation, leading to a higher energy threshold of 100 TeV. Three events were found over a background prediction of 0.04 atmospheric muon events and 0.21 events from the flux of conventional and prompt atmospheric neutrinos. Including systematic errors this corresponds to a 2.7 sigma excess with respect to the background-only hypothesis. Our observation of neutrino event candidates above 100 TeV complements IceCube's recently observed evidence for high-energy astrophysical neutrinos.
C1 [Bissok, M.; Blumenthal, J.; Coenders, S.; Euler, S.; Gretskov, P.; Hallen, P.; Heinen, D.; Jagielski, K.; Kriesten, A.; 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, Inst Phys 3, D-52056 Aachen, Germany.
[Aartsen, M. G.; Hill, G. C.; Robertson, S.; Whelan, B.] 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.
[de With, M.; Kolanoski, H.; Waldenmaier, T.] Univ Berlin, Inst Phys, D-12489 Berlin, Germany.
[Tjus, J. Becker; Eichmann, B.; Fedynitch, A.; Saba, S. M.; Schoeneberg, S.; Unger, E.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Boeser, S.; Franckowiak, A.; Hebecker, D.; Homeier, A.; Kowalski, M.; Schulte, L.; Stasik, A.; Strotjohann, N. L.; Usner, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Brussels, Sci Fac CP230, B-1050 Brussels, Belgium.
[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.; Macias, O.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Berley, D.; Blaufuss, E.; Christy, B.; 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.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, 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.
[Koskinen, D. J.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[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.
[Grandmont, D. T.; Grant, D.; Nowicki, S. C.; Odrowski, S.; Sheremata, C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Altmann, D.; Classen, L.; Gora, D.; Kappes, A.; Tselengidou, M.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91054 Erlangen, Germany.
[Aguilar, J. A.; Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[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.; Arguelles, C.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; 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.; Tobin, M. N.; 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.; Arguelles, C.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; 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.; Tobin, M. N.; 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.] Univ Delaware, Bartol Res Inst, 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.] Univ Delaware, Dept Phys & Astron, 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.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Bose, D.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
[Clark, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Larson, M. J.; Palczewski, T.; 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.
[Arlen, T. C.; Boersma, D. J.; Cowen, D. F.; de Andre, J. P. A. M.; DeYoung, T.; Dunkman, M.; Eagan, R.; Groh, J. C.; Huang, F.; Quinnan, M.; Smith, M. W. E.; Stanisha, N. A.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Botner, O.; Hallgren, A.; Perez de los Heros, C.; 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.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Jacobi, E.; Kaminsky, B.; Karg, T.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Spiering, C.; Stossl, A.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hickford, S (reprint author), Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch 1, New Zealand.
EM stephanie.v.hickford@gmail.com; eike.middell@desy.de
RI Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty,
James/D-9310-2011; Wiebusch, Christopher/G-6490-2012; Tjus,
Julia/G-8145-2012; Koskinen, David/G-3236-2014; Auffenberg,
Jan/D-3954-2014; Aguilar Sanchez, Juan Antonio/H-4467-2015; Taavola,
Henric/B-4497-2011;
OI Maruyama, Reina/0000-0003-2794-512X; Sarkar, Subir/0000-0002-3542-858X;
Beatty, James/0000-0003-0481-4952; Wiebusch,
Christopher/0000-0002-6418-3008; Rott, Carsten/0000-0002-6958-6033;
Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft,
Anne/0000-0002-9112-5479; Groh, John/0000-0001-9880-3634; Koskinen,
David/0000-0002-0514-5917; Auffenberg, Jan/0000-0002-1185-9094; Aguilar
Sanchez, Juan Antonio/0000-0003-2252-9514; Taavola,
Henric/0000-0002-2604-2810; Perez de los Heros,
Carlos/0000-0002-2084-5866; Strotjohann, Nora Linn/0000-0002-4667-6730;
Arguelles Delgado, Carlos/0000-0003-4186-4182
FU U.S. National Science Foundation-Office of Polar Programs; U.S. National
Science Foundation-Physics Division; University of Wisconsin Alumni
Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid
infrastructure at the University of Wisconsin-Madison; Open Science Grid
(OSG) grid infrastructure; U.S. Department of Energy; National Energy
Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI) grid computing resources; Natural Sciences and
Engineering Research Council of Canada; WestGrid and Compute/Calcul
Canada; Swedish Research Council; Swedish Polar Research Secretariat;
Swedish National Infrastructure for Computing (SNIC),; Knut and Alice
Wallenberg Foundation, Sweden; German Ministry for Education and
Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Helmholtz
Alliance for Astroparticle Physics (HAP); Research Department of Plasmas
with Complex Interactions (Bochum), Germany; Fund for Scientific
Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to
encourage scientific and technological research in industry (IWT);
Belgian Federal Science Policy Office (Belspo); University of Oxford,
United Kingdom; Marsden Fund, New Zealand; Australian Research Council;
Japan Society for Promotion of Science (JSPS); Swiss National Science
Foundation (SNSF), Switzerland; National Research Foundation of Korea
(NRF); Danish National Research Foundation, Denmark (DNRF)
FX We acknowledge the support from the following agencies: U.S. National
Science Foundation-Office of Polar Programs, U.S. National Science
Foundation-Physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid
infrastructure; U.S. Department of Energy, and National Energy Research
Scientific Computing Center, the Louisiana Optical Network Initiative
(LONI) grid computing resources; Natural Sciences and Engineering
Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish
Research Council, Swedish Polar Research Secretariat, Swedish National
Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg
Foundation, Sweden; German Ministry for Education and Research (BMBF),
Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for
Astroparticle Physics (HAP), Research Department of Plasmas with Complex
Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO),
FWO Odysseus programme, Flanders Institute to encourage scientific and
technological research in industry (IWT), Belgian Federal Science Policy
Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New
Zealand; Australian Research Council; Japan Society for Promotion of
Science (JSPS); the Swiss National Science Foundation (SNSF),
Switzerland; National Research Foundation of Korea (NRF); Danish
National Research Foundation, Denmark (DNRF)
NR 58
TC 17
Z9 17
U1 0
U2 8
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD MAY 1
PY 2014
VL 89
IS 10
AR 102001
DI 10.1103/PhysRevD.89.102001
PG 20
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AG6LZ
UT WOS:000335531400002
ER
PT J
AU de Putter, R
Linder, EV
Mishra, A
AF de Putter, Roland
Linder, Eric V.
Mishra, Abhilash
TI Inflationary freedom and cosmological neutrino constraints
SO PHYSICAL REVIEW D
LA English
DT Article
ID PRIMORDIAL POWER SPECTRUM; OSCILLATION SPECTROSCOPIC SURVEY;
MICROWAVE-ANISOTROPY-PROBE; COSMIC INVERSION METHOD; SOUTH-POLE
TELESCOPE; DIGITAL SKY SURVEY; SDSS-III; BACKGROUND ANISOTROPIES; WMAP
OBSERVATIONS; DATA RELEASE
AB The most stringent bounds on the absolute neutrino mass scale come from cosmological data. These bounds are made possible because massive relic neutrinos affect the expansion history of the universe and lead to a suppression of matter clustering on scales smaller than the associated free streaming length. However, the resulting effect on cosmological perturbations is relative to the primordial power spectrum of density perturbations from inflation, so freedom in the primordial power spectrum affects neutrino mass constraints. Using measurements of the cosmic microwave background (CMB), the galaxy power spectrum and the Hubble constant, we constrain neutrino mass and number of species for a model-independent primordial power spectrum. Describing the primordial power spectrum by a 20-node spline, we find that the neutrino mass upper limit is a factor 3 weaker than when a power law form is imposed, if only CMB data are used. The primordial power spectrum itself is constrained to better than 10% in the wave vector range k approximate to 0.01 - 0.25 Mpc(-1). Galaxy clustering data and a determination of the Hubble constant play a key role in reining in the effects of inflationary freedom on neutrino constraints. The inclusion of both eliminates the inflationary freedom degradation of the neutrino mass bound, giving for the sum of neutrino masses Sigma m(nu) < 0.18 eV (at 95% confidence level, Planck + BOSS + H-0), approximately independent of the assumed primordial power spectrum model. When allowing for a free effective number of species, N-eff, the joint constraints on Sigma m(nu) and N-eff are loosened by a factor 1.7 when the power law form of the primordial power spectrum is abandoned in favor of the spline parametrization.
C1 [de Putter, Roland] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[de Putter, Roland; Mishra, Abhilash] CALTECH, Pasadena, CA 91125 USA.
[Linder, Eric V.] Univ Calif Berkeley, Berkeley Lab, Berkeley, CA 94720 USA.
[Linder, Eric V.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Linder, Eric V.] Ewha Womans Univ, Inst Early Universe WCU, Seoul 120750, South Korea.
RP de Putter, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU NASA ATP [11-ATP090]; DOE Grant [DE-SC-0007867]; Director, Office of
Science, Office of High Energy Physics; U.S. Department of Energy
[DE-AC02-05CH11231]; Korea World Class University [R32-2009-000-10130-0]
FX We thank Olga Mena for her assistance with the galaxy power spectrum
likelihood code and Jan Hamann for useful discussion regarding Appendix
B. 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. This
work is supported by NASA ATP Grant No. 11-ATP090, DOE Grant No.
DE-SC-0007867, and the Director, Office of Science, Office of High
Energy Physics, of the U.S. Department of Energy under Contract No.
DE-AC02-05CH11231, and by Korea World Class University Grant No.
R32-2009-000-10130-0. R. d. P. thanks the Institute for the Early
Universe at Ewha University, Seoul, where part of this work was
performed, for its hospitality.
NR 68
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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 MAY 1
PY 2014
VL 89
IS 10
AR 103502
DI 10.1103/PhysRevD.89.103502
PG 17
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AG6LZ
UT WOS:000335531400005
ER
PT J
AU Min, JB
Xue, D
Shi, Y
AF Min, J. B.
Xue, D.
Shi, Y.
TI Micromechanics modeling for fatigue damage analysis designed for fabric
reinforced ceramic matrix composites
SO COMPOSITE STRUCTURES
LA English
DT Article
DE Three-phase micromechanics; Shear-lag; Fracture mechanics; Damage
progression; Fatigue failure; Fabric reinforced composite structures
ID FIBER; FRACTURE; FAILURE
AB A micromechanics analysis modeling method was developed to analyze the damage progression and fatigue failure of fabric reinforced composite structures, especially for the brittle ceramic matrix material composites. A repeating unit cell concept of fabric reinforced composites was used to represent the global composite structure. The thermal and mechanical properties of the repeating unit cell were considered as the same as those of the global composite structure. The three-phase micromechanics, the shear-lag, and the continuum fracture mechanics models were integrated with a statistical model in the repeating unit cell to predict the progressive damages and fatigue life of the composite structures. The global structure failure was defined as the loss of loading capability of the repeating unit cell, which depends on the stiffness reduction due to material slice failures and nonlinear material properties in the repeating unit cell. The present methodology is demonstrated with the analysis results evaluated through the experimental test performed with carbon fiber reinforced silicon carbide matrix plain weave composite specimens. Published by Elsevier Ltd.
C1 [Min, J. B.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Xue, D.; Shi, Y.] Analyt Serv & Mat Inc, Hampton, VA 23666 USA.
RP Min, JB (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
EM James.B.Min@nasa.gov
FU NASA Fundamental Aeronautics Research Fixed Wing Project
FX The first author gratefully acknowledges the support by NASA Fundamental
Aeronautics Research Fixed Wing Project to prepare this paper.
NR 25
TC 4
Z9 6
U1 2
U2 19
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0263-8223
EI 1879-1085
J9 COMPOS STRUCT
JI Compos. Struct.
PD MAY
PY 2014
VL 111
BP 213
EP 223
DI 10.1016/j.compstruct.2013.12.025
PG 11
WC Materials Science, Composites
SC Materials Science
GA AG5VN
UT WOS:000335486900021
ER
PT J
AU Liu, Z
Ostrenga, D
Teng, W
Kempler, S
Milich, L
AF Liu, Zhong
Ostrenga, Dana
Teng, William
Kempler, Steven
Milich, Lenard
TI Developing GIOVANNI-based online prototypes to intercompare TRMM-related
global gridded-precipitation products
SO COMPUTERS & GEOSCIENCES
LA English
DT Article
DE Precipitation; Satellite remote sensing; Intercomparison; Uncertainty;
TRMM; Online tools
ID TROPICAL RAINFALL; PASSIVE MICROWAVE; ORBIT BOOST; SATELLITE; SYSTEM;
VISUALIZATION; VALIDATION; RESOLUTION; ALGORITHM; INFORMATION
AB New online prototypes have been developed to extend and enhance the previous effort by facilitating investigation of product characteristics and intercomparison of precipitation products in different algorithms as well as in different versions at different spatial scales ranging from local to global without downloading data and software. Several popular Tropical Rainfall Measuring Mission (TRMM) products and the TRMM Composite Climatology are included. In addition, users can download customized data in several popular formats for further analysis. Examples show product quality problems and differences in several monthly precipitation products. It is seen that differences in daily and monthly precipitation products are distributed unevenly in space and it is necessary to have tools such as those presented here for customized and detailed investigations. A simple time series and two area maps allow the discovery of abnormal values of 3A25 in one of the months. An example shows a V-shaped valley issue in the Version 6 3B43 time series and another example shows a sudden drop in 3A25 monthly rain rate, all of which provide important information when the products are used for long-term trend studies. Future plans include adding more products and statistical functionality in the prototypes. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Liu, Zhong; Ostrenga, Dana; Teng, William; Kempler, Steven] NASA Goddard Space Flight Ctr, Goddard Earth Sci Data & Informat Serv Ctr GES DI, Greenbelt, MD 20771 USA.
[Liu, Zhong] George Mason Univ, CSISS, Fairfax, VA 22030 USA.
[Ostrenga, Dana; Teng, William] ADNET Syst Inc, Rockville, MD USA.
[Milich, Lenard] Univ Arizona, Tucson, AZ 85721 USA.
RP Liu, Z (reprint author), NASA Goddard Space Flight Ctr, Goddard Earth Sci Data & Informat Serv Ctr GES DI, Code 610-2, Greenbelt, MD 20771 USA.
EM Zhong.Liu@nasa.gov
FU NASA Research Opportunities in Space and Earth Science (ROSES); NASA GES
DISC; Earth System Data Records Uncertainty Analysis;
[NNH10ZDA001N-ESDRERR]
FX This project is supported by NASA Research Opportunities in Space and
Earth Science-2010 (ROSES-2010), NNH10ZDA001N-ESDRERR, Appendix A32:
"Earth System Data Records Uncertainty Analysis" and the NASA GES DISC.
Special thanks to the GIOVANNI development team and Dr. Jianfu Pan for
providing the details about the Giovanni infrastructure. Thanks extend
to Drs. Robert Adler and Jian-Jian Wang for providing the TCC products
and the description and participating in the tool development The
authors would like to thank three anonymous reviewers for their
constructive comments, which have much improved the manuscript
NR 29
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U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0098-3004
EI 1873-7803
J9 COMPUT GEOSCI-UK
JI Comput. Geosci.
PD MAY
PY 2014
VL 66
BP 168
EP 181
DI 10.1016/j.cageo.2013.12.012
PG 14
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA AG3CP
UT WOS:000335293700016
ER
PT J
AU Duan, L
Choudhari, MM
Wu, MW
AF Duan, Lian
Choudhari, Meelan M.
Wu, Minwei
TI Numerical study of acoustic radiation due to a supersonic turbulent
boundary layer
SO JOURNAL OF FLUID MECHANICS
LA English
DT Article
DE aeroacoustics; turbulent boundary layers; turbulence simulation
ID WALL-PRESSURE-FLUCTUATIONS; CHANNEL FLOW; REYNOLDS-NUMBER; SHEAR FLOWS;
SIMULATION; TRANSITION; FIELD; BENEATH; NOISE; RECEPTIVITY
AB Direct numerical simulations are used to examine the pressure fluctuations generated by fully developed turbulence in a Mach 2.5 turbulent boundary layer, with an emphasis on the acoustic fluctuations radiated into the free stream. Single-and multi-point statistics of computed surface pressure fluctuations show good agreement with measurements and numerical simulations at similar flow conditions. Consistent with spark shadowgraphs obtained in free flight, the quasi-homogeneous acoustic near field in the free-stream region consists of randomly spaced wavepackets with a finite spatial coherence. The free-stream pressure fluctuations exhibit important differences from the surface pressure fluctuations in amplitude, frequency content and convection speeds. Such information can be applied towards improved modelling of boundary layer receptivity in conventional supersonic facilities and, hence, enable a better utilization of transition data acquired in such wind tunnels. The predicted acoustic characteristics are compared with the limited available measurements. Finally, the numerical database is used to understand the acoustic source mechanisms, with the finding that the supersonically convecting eddies that can directly radiate to the free stream are confined to the buffer zone within the boundary layer.
C1 [Duan, Lian] Missouri Univ Sci & Technol, Rolla, MO 65409 USA.
[Choudhari, Meelan M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Wu, Minwei] Natl Inst Aerosp, Hampton, VA 23666 USA.
RP Duan, L (reprint author), Missouri Univ Sci & Technol, Rolla, MO 65409 USA.
EM duanl@mst.edu
RI Choudhari, Meelan/F-6080-2017
OI Choudhari, Meelan/0000-0001-9120-7362
NR 62
TC 2
Z9 2
U1 1
U2 23
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0022-1120
EI 1469-7645
J9 J FLUID MECH
JI J. Fluid Mech.
PD MAY
PY 2014
VL 746
BP 165
EP 192
DI 10.1017/jfm.2014.116
PG 28
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA AG4IW
UT WOS:000335384200012
ER
PT J
AU Joshi, SM
Gonzalez, OR
Upchurch, JM
AF Joshi, Suresh M.
Gonzalez, Oscar R.
Upchurch, Jason M.
TI Identifiability of Additive Actuator and Sensor Faults by State
Augmentation
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
C1 [Joshi, Suresh M.; Upchurch, Jason M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Gonzalez, Oscar R.] Old Dominion Univ, Dept Elect & Comp Engn, Norfolk, VA 23529 USA.
RP Joshi, SM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM suresh.m.joshi@nasa.gov; ogonzale@odu.edu; jason.m.upchurch@nasa.gov
FU Copyright Clearance Center, Inc.
FX This material is declared a work of the U.S. Government and is not
subject to copyright protection in the United States. Copies of this
paper may be made for personal or internal use, on condition that the
copier pay the $ 10.00 per-copy fee to the Copyright Clearance Center,
Inc., 222 Rosewood Drive, Danvers, MA 01923; include the code
1533-3884/14 and $ 10.00 in correspondence with the CCC.
NR 11
TC 1
Z9 1
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD MAY-JUN
PY 2014
VL 37
IS 3
BP 941
EP 946
DI 10.2514/1.62523
PG 6
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA AG4NT
UT WOS:000335397700021
ER
PT J
AU Neichel, B
Rigaut, F
Vidal, F
van Dam, MA
Garrel, V
Carrasco, ER
Pessev, P
Winge, C
Boccas, M
d'Orgeville, C
Arriagada, G
Serio, A
Fesquet, V
Rambold, WN
Luhrs, J
Moreno, C
Gausachs, G
Galvez, RL
Montes, V
Vucina, TB
Marin, E
Urrutia, C
Lopez, A
Diggs, SJ
Marchant, C
Ebbers, AW
Trujillo, C
Bec, M
Trancho, G
McGregor, P
Young, PJ
Colazo, F
Edwards, ML
AF Neichel, Benoit
Rigaut, Francois
Vidal, Fabrice
van Dam, Marcos A.
Garrel, Vincent
Rodrigo Carrasco, Eleazar
Pessev, Peter
Winge, Claudia
Boccas, Maxime
d'Orgeville, Celine
Arriagada, Gustavo
Serio, Andrew
Fesquet, Vincent
Rambold, William N.
Luehrs, Javier
Moreno, Cristian
Gausachs, Gaston
Galvez, Ramon L.
Montes, Vanessa
Vucina, Tomislav B.
Marin, Eduardo
Urrutia, Cristian
Lopez, Ariel
Diggs, Sarah J.
Marchant, Claudio
Ebbers, Angelic W.
Trujillo, Chadwick
Bec, Matthieu
Trancho, Gelys
McGregor, Peter
Young, Peter J.
Colazo, Felipe
Edwards, Michelle L.
TI Gemini multiconjugate adaptive optics system review - II. Commissioning,
operation and overall performance
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE instrumentation: adaptive optics; instrumentation: high angular
resolution; telescopes
ID LASER-GUIDE-STAR; CENTROID GAIN; BLACK-HOLE; FIELD; GALAXIES; SOUTH;
COMPENSATION; MITIGATION; TELESCOPES; DYNAMICS
AB The Gemini multiconjugate adaptive optics system - GeMS, a facility instrument mounted on the Gemini South telescope, delivers a uniform, near diffraction limited images at near-infrared wavelengths (0.95-2.5 mu m) over a field of view of 120 arcsec. GeMS is the first sodium layer based multilaser guide star adaptive optics system used in astronomy. It uses five laser guide stars distributed on a 60 arcsec square constellation to measure for atmospheric distortions and two deformable mirrors to compensate for it. In this paper, the second one devoted to describe the GeMS project, we present the commissioning, overall performance and operational scheme of GeMS. Performance of each subsystem is derived from the commissioning results. The typical image quality, expressed in full with at half-maximum, Strehl ratios and variations over the field delivered by the system are then described. A discussion of the main contributor to performance limitation is carried out. Finally, overheads and future system upgrades are described.
C1 [Neichel, Benoit; Vidal, Fabrice; van Dam, Marcos A.; Garrel, Vincent; Rodrigo Carrasco, Eleazar; Pessev, Peter; Winge, Claudia; Boccas, Maxime; Arriagada, Gustavo; Serio, Andrew; Fesquet, Vincent; Rambold, William N.; Luehrs, Javier; Moreno, Cristian; Gausachs, Gaston; Galvez, Ramon L.; Montes, Vanessa; Vucina, Tomislav B.; Marin, Eduardo; Urrutia, Cristian; Lopez, Ariel; Diggs, Sarah J.; Marchant, Claudio; Ebbers, Angelic W.; Trujillo, Chadwick] AURA, Gemini Observ, La Serena, Chile.
[Neichel, Benoit] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Rigaut, Francois; d'Orgeville, Celine; McGregor, Peter; Young, Peter J.] Australian Natl Univ, RSAA, Mt Stromlo Observ, Weston, ACT 2611, Australia.
[van Dam, Marcos A.] Flat Wavefronts, Christchurch 8140, New Zealand.
[Bec, Matthieu; Trancho, Gelys] Giant Magellan Telescope Org Corp, Pasadena, CA 91109 USA.
[Colazo, Felipe] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Edwards, Michelle L.] Univ Arizona, LBT Observ, Tucson, AZ 85721 USA.
RP Neichel, B (reprint author), AURA, Gemini Observ, Casilla 603, La Serena, Chile.
EM benoit.neichel@lam.fr
FU French ANR programme WASABI [ANR-13-PDOC-0006-01]
FX Part of this work has been funded by the French ANR programme WASABI -
ANR-13-PDOC-0006-01.
NR 63
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U1 2
U2 15
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 MAY
PY 2014
VL 440
IS 2
BP 1002
EP 1019
DI 10.1093/mnras/stu403
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF5GO
UT WOS:000334742200005
ER
PT J
AU Komarov, SV
Churazov, EM
Schekochihin, AA
ZuHone, JA
AF Komarov, S. V.
Churazov, E. M.
Schekochihin, A. A.
ZuHone, J. A.
TI Suppression of local heat flux in a turbulent magnetized intracluster
medium
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE conduction; magnetic fields; plasmas; turbulence; galaxies: clusters:
intracluster medium
ID ANISOTROPIC THERMAL CONDUCTION; GALAXY CLUSTERS; COLD FRONTS; BUOYANCY
INSTABILITIES; X-RAY; MAGNETOHYDRODYNAMIC SIMULATIONS; GAS MOTIONS;
FIELDS; TRANSPORT; PROFILES
AB X-ray observations of hot gas in galaxy clusters often show steeper temperature gradients across cold fronts - contact discontinuities, driven by the differential gas motions. These sharp (a few kpc wide) surface brightness/temperature discontinuities would be quickly smeared out by the electron thermal conduction in unmagnetized plasma, suggesting significant suppression of the heat flow across the discontinuities. In fact, the character of the gas flow near cold fronts is favourable for suppression of conduction by aligning magnetic field lines along the discontinuities. We argue that a similar mechanism is operating in the bulk of the gas. Generic 3D random isotropic and incompressible motions increase the temperature gradients (in some places) and at the same time suppress the local conduction by aligning the magnetic field lines perpendicular to the local temperature gradient. We show that the suppression of the effective conductivity in the bulk of the gas can be linked to the increase of the frozen magnetic field energy density. On average the rate of decay of the temperature fluctuations d <>/dt decreases as << B-2 >>(-1/5).
C1 [Komarov, S. V.; Churazov, E. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Komarov, S. V.; Churazov, E. M.] Space Res Inst IKI, Moscow 117997, Russia.
[Komarov, S. V.] MIPT, Inst Pereulok 9, Dolgoprudnyi 141700, Moscow Region, Russia.
[Schekochihin, A. A.] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England.
[ZuHone, J. A.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
RP Komarov, SV (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
EM komarov@mpa-garching.mpg.de
RI Churazov, Eugene/A-7783-2013
FU Leverhulme Trust Network on Magnetized Plasma Turbulence
FX This work was supported in part by the Leverhulme Trust Network on
Magnetized Plasma Turbulence.
NR 51
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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 MAY
PY 2014
VL 440
IS 2
BP 1153
EP 1164
DI 10.1093/mnras/stu281
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF5GO
UT WOS:000334742200016
ER
PT J
AU Agliozzo, C
Noriega-Crespo, A
Umana, G
Flagey, N
Buemi, C
Ingallinera, A
Trigilio, C
Leto, P
AF Agliozzo, C.
Noriega-Crespo, A.
Umana, G.
Flagey, N.
Buemi, C.
Ingallinera, A.
Trigilio, C.
Leto, P.
TI The candidate luminous blue variable G79.29+0.46: a comprehensive study
of its ejecta through a multiwavelength analysis
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: early-type; stars: evolution; stars: mass-loss; ISM: bubbles;
infrared: ISM; radio continuum: ISM
ID LARGE ARRAY OBSERVATIONS; RING NEBULA G79.29+0.46;
LARGE-MAGELLANIC-CLOUD; H-II REGIONS; ETA-CARINAE; CYGNUS-X;
GALACTIC-CENTER; MU-M; SPITZER; DUST
AB We present a multiwavelength analysis of the nebula around the candidate luminous blue variable G79.29+0.46. The study is based on our radio observations performed at the Expanded Very Large Array and at the Green Bank Telescope and on archival infrared data sets, including recent images obtained by the Herschel Space Observatory. We confirm that the radio central object is characterized by a stellar wind and we derive a current mass-loss rate of about 1.4 x 10(-6) M-circle dot yr(-1). We find the presence of a dusty compact envelope close to the star, with a temperature between similar to 40 and 1200 K. We estimate for the outer ejecta an ionized gas mass of 1.51 M-circle dot and a warm (60-85 K) dust mass of 0.02 M-circle dot. Diagnostics of the far-infrared spectra indicate the presence of a photodissociation region around the ionized gas. Finally, we model the nebula with the photoionization code cloudy, using as input parameters those estimated from our analysis. We find for the central star a luminosity of 10(5.4) L-circle dot and an effective temperature of 20.4 kK.
C1 [Agliozzo, C.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile.
[Agliozzo, C.] Univ Catania, Sez Astrofis, Dipartimento Fis & Astron, I-95123 Catania, Italy.
[Noriega-Crespo, A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Umana, G.; Buemi, C.; Ingallinera, A.; Trigilio, C.; Leto, P.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Flagey, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Agliozzo, C (reprint author), Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile.
EM agliozzo@oact.inaf.it
OI Buemi, Carla Simona/0000-0002-7288-4613; Umana,
Grazia/0000-0002-6972-8388; Leto, Paolo/0000-0003-4864-2806
FU NASA; ESA Member States; National Science Foundation
FX This work is based on observations performed at the National Radio
Astronomy Observatory, a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
Herschel is a European Space Agency (ESA) space observatory with science
instruments provided by the European-led Principal Investigator
consortia and with important participation from the National Aeronautics
and Space Administration (NASA). This research has also made use of the
NASA/IPAC Infrared Science Archive, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA. The ISO was an ESA project with instruments funded
by ESA Member States (especially the PI countries, France, Germany, the
Netherlands and the UK) and with the participation of ISAS and NASA.
Finally, this publication makes use of data products from the 2MASS,
which is a joint project of the University of Massachusetts and the
Infrared Processing and Analysis Center/California Institute of
Technology, funded by NASA and the National Science Foundation.
NR 70
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U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2014
VL 440
IS 2
BP 1391
EP 1409
DI 10.1093/mnras/stu296
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF5GO
UT WOS:000334742200034
ER
PT J
AU Vigeland, SJ
Vallisneri, M
AF Vigeland, Sarah J.
Vallisneri, Michele
TI Bayesian inference for pulsar-timing models
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational waves
ID GRAVITATIONAL-RADIATION; MILLISECOND PULSARS; LIMITS; PACKAGE; BINARY;
TEMPO2; ASTROMETRY; SYSTEM; WAVES; NOISE
AB The extremely regular, periodic radio emission from millisecond pulsars makes them useful tools for studying neutron star astrophysics, general relativity, and low-frequency gravitational waves. These studies require that the observed pulse times of arrival be fitted to complex timing models that describe numerous effects such as the astrometry of the source, the evolution of the pulsar's spin, the presence of a binary companion, and the propagation of the pulses through the interstellar medium. In this paper, we discuss the benefits of using Bayesian inference to obtain pulsar-timing solutions. These benefits include the validation of linearized least-squares model fits when they are correct, and the proper characterization of parameter uncertainties when they are not; the incorporation of prior parameter information and of models of correlated noise; and the Bayesian comparison of alternative timing models. We describe our computational setup, which combines the timing models of tempo2 with the nested-sampling integrator multinest. We compare the timing solutions generated using Bayesian inference and linearized least-squares for three pulsars: B1953+29, J2317+1439, and J1640+2224, which demonstrate a variety of the benefits that we posit.
C1 [Vigeland, Sarah J.; Vallisneri, Michele] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Vigeland, SJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Sarah.J.Vigeland@jpl.nasa.gov; Michele.Vallisneri@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA) Postdoctoral
Programme at the Jet Propulsion Laboratory; NASA; Jet Propulsion
Laboratory RTD Programme
FX We are grateful to Paul Demorest, Joe Lazio, Sarah Burke-Spolaor, Rutger
van Haasteren, Lindley Lentati, Tom Prince, and to all NANOGrav
colleagues for helpful discussions. SV was supported by an appointment
to the National Aeronautics and Space Administration (NASA) Postdoctoral
Programme at the Jet Propulsion Laboratory administered by Oak Ridge
Associated Universities through a contract with NASA. MV was supported
by the Jet Propulsion Laboratory RTD Programme. This work was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under contract to the NASA. Copyright 2014 California
Institute of Technology.
NR 48
TC 8
Z9 8
U1 1
U2 7
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 MAY
PY 2014
VL 440
IS 2
BP 1446
EP 1457
DI 10.1093/mnras/stu312
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF5GO
UT WOS:000334742200038
ER
PT J
AU Giocoli, C
Meneghetti, M
Metcalf, RB
Ettori, S
Moscardini, L
AF Giocoli, Carlo
Meneghetti, Massimo
Metcalf, R. Benton
Ettori, Stefano
Moscardini, Lauro
TI Mass and concentration estimates from weak and strong gravitational
lensing: a systematic study
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: strong; gravitational lensing: weak; methods:
analytical; galaxies: haloes; cosmology: theory; dark matter
ID DARK-MATTER HALOS; HIERARCHICAL SATELLITE ACCRETION; SIMULATED GALAXY
CLUSTERS; X-RAY-CLUSTERS; MARENOSTRUM UNIVERSE; DENSITY PROFILE; ARC
STATISTICS; SUBSTRUCTURE; SHAPES; MODELS
AB We study how well halo properties of galaxy clusters, such as mass and concentration, are recovered using lensing data. In order to generate a large sample of systems at different redshifts, we use the code moka. We measure halo mass and concentration using weak lensing data alone (WL), fitting to a Navarro, Frenk & White (NFW) profile the reduced tangential shear profile, or by combining weak and strong lensing data, by adding information about the size of the Einstein radius (WL+SL). For different redshifts, we measure the mass and the concentration biases and find that these are mainly caused by the random orientation of the halo ellipsoid with respect to the line of sight. Since our simulations account for the presence of a bright central galaxy, we perform mass and concentration measurements using a generalized NFW profile which allows for a free inner slope. This reduces both the mass and the concentration biases. We discuss how the mass function and the concentration-mass relation change when using WL and WL+SL estimates. We investigate how selection effects impact the measured concentration-mass relation showing that strong lens clusters may have a concentration 20-30 per cent higher than the average, at fixed mass, considering also the particular case of strong lensing selected samples of relaxed clusters. Finally, we notice that selecting a sample of relaxed galaxy clusters, as is done in some cluster surveys, explains the concentration-mass relation biases.
C1 [Giocoli, Carlo; Metcalf, R. Benton; Moscardini, Lauro] Alma Mater Studiorum Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy.
[Giocoli, Carlo; Meneghetti, Massimo; Ettori, Stefano; Moscardini, Lauro] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Giocoli, Carlo; Meneghetti, Massimo; Ettori, Stefano; Moscardini, Lauro] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy.
[Meneghetti, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Giocoli, C (reprint author), Alma Mater Studiorum Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
EM carlo.giocoli@unibo.it
RI Ettori, Stefano/N-5004-2015; Meneghetti, Massimo/O-8139-2015;
OI Ettori, Stefano/0000-0003-4117-8617; Meneghetti,
Massimo/0000-0003-1225-7084; METCALF, ROBERT BENTON/0000-0003-3167-2574
FU project GLENCO under European Seventh Framework Programme, Ideas
[259349]; PRIN MIUR; PRIN-INAF; MOKALEN3 [HP10CMXLBH];
[ASI/INAFI/023/12/0]; [ASI-INAF I/088/06/0]
FX CG and RBM's research is part of the project GLENCO, funded under the
European Seventh Framework Programme, Ideas, Grant Agreement no. 259349.
We acknowledge financial contributions from contracts ASI/INAFI/023/12/0
and by the PRIN MIUR 2010-2011 'The dark Universe and the cosmic
evolution of baryons: from current surveys to Euclid'. CG and LM also
acknowledge the financial contribution by the PRIN INAF 2012 'The
Universe in the box: multiscale simulations of cosmic structure'. SE
acknowledges the financial contribution from contracts ASI-INAF
I/088/06/0 and PRIN-INAF 2012. CG would like to thank Giuseppe Tormen
and Vincenzo Mezzalira to have host part of the computer jobs run to
produce the simulated galaxy cluster sample. Part of the simulations of
this project have been run during the Class C Project-HP10CMXLBH
(MOKALEN3). CG would also like to particularly thank Matthias Bartelmann
for useful and stimulating discussions. We are also grateful to Marusa
Bradac Anja Von der Linden, Stefano Borgani, Stefano Andreon and Mauro
Sereno for the conversations they had during the conference in Madonna
di Campiglio in 2013 March. We are grateful to the anonymous referee for
his/her comments and suggestions that helped to improve the presentation
of our results.
NR 86
TC 15
Z9 15
U1 0
U2 2
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 MAY
PY 2014
VL 440
IS 2
BP 1899
EP 1915
DI 10.1093/mnras/stu303
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF5GO
UT WOS:000334742200071
ER
PT J
AU Prive, NC
Errico, RM
Tai, KS
AF Prive, N. C.
Errico, R. M.
Tai, K. -S.
TI The Impact of Increased Frequency of Rawinsonde Observations on Forecast
Skill Investigated with an Observing System Simulation Experiment
SO MONTHLY WEATHER REVIEW
LA English
DT Article
DE Radiosonde observations; Numerical weather prediction/forecasting;
Forecast verification/skill
ID DATA ASSIMILATION SYSTEM; MOIST PHYSICS; VALIDATION; OFFICE
AB Most rawinsondes are launched once or twice daily, at 0000 and/or 1200 UTC; only a small number of the total rawinsonde observations are taken at 0600 and 1800 UTC ("off hour" cycle times). In this study, the variations of forecast and analysis quality between cycle times and the potential improvement of skill due to supplemental rawinsonde measurements at 0600 and 1800 UTC are tested in the framework of an observing system simulation experiment (OSSE). The National Aeronautics and Space Administration Global Modeling and Assimilation Office (NASA GMAO) Goddard Earth Observing System Model, version 5 (GEOS-5), is used with the GMAO OSSE setup for an experiment emulating the months of July and August with the 2011 observational network. The OSSE is run with and without supplemental rawinsonde observations at 0600 and 1800 UTC, and the differences in analysis error and forecast skill are quantified. The addition of supplemental rawinsonde observations results in significant improvement of analysis quality in the Northern Hemisphere for both the 0000/1200 and 0600/1800 UTC cycle times, with greater improvement for the off-hour times. Reduction of root-mean-square errors on the order of 1%-3% for wind and temperature is found at the 24- and 48-h forecast times. There is a slight improvement in Northern Hemisphere anomaly correlations at the 120-h forecast time.
C1 [Prive, N. C.; Errico, R. M.] Morgan State Univ, Goddard Earth Sci Technol & Res Ctr, Greenbelt, MD USA.
[Tai, K. -S.] Sci Syst & Applicat Inc, Greenbelt, MD USA.
RP Prive, NC (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM nikki.prive@nasa.gov
OI Prive, Nikki/0000-0001-8309-8741
FU GMAO
FX The ECMWF nature run was provided by Erik Andersson through arrangements
made by Michiko Masutani. Support for this project was encouraged by
Michele Rienecker and provided by GMAO core funding. Helpful comments
from three anonymous reviewers led to significant improvements in this
manuscript.
NR 12
TC 2
Z9 2
U1 1
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD MAY
PY 2014
VL 142
IS 5
BP 1823
EP 1834
DI 10.1175/MWR-D-13-00237.1
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AG0OS
UT WOS:000335115400008
ER
PT J
AU Zhou, LM
Tian, YH
Myneni, RB
Ciais, P
Saatchi, S
Liu, YY
Piao, SL
Chen, HS
Vermote, EF
Song, CH
Hwang, TH
AF Zhou, Liming
Tian, Yuhong
Myneni, Ranga B.
Ciais, Philippe
Saatchi, Sassan
Liu, Yi Y.
Piao, Shilong
Chen, Haishan
Vermote, Eric F.
Song, Conghe
Hwang, Taehee
TI Widespread decline of Congo rainforest greenness in the past decade
SO NATURE
LA English
DT Article
ID VEGETATION INDEXES; MICROWAVE EMISSION; TROPICAL FORESTS; DRY SEASON;
MODIS; DROUGHT; CLIMATE; AMAZON; RETRIEVALS; PRODUCTS
AB Tropical forests are global epicentres of biodiversity and important modulators of climate change(1), and are mainly constrained by rainfall patterns(1-3). The severe short-term droughts that occurred recently in Amazonia have drawn attention to the vulnerability of tropical forests to climatic disturbances(4-9). The central African rainforests, the second-largest on Earth, have experienced a long-term drying trend(10,11) whose impacts on vegetation dynamics remain mostly unknown because in situ observations are very limited. The Congolese forest, with its drier conditions and higher percentage of semi-evergreen trees(12,13), may be more tolerant to short-term rainfall reduction than are wetter tropical forests(11), but for a long-term drought there may be critical thresholds of water availability below which higher-biomass, closed-canopy forests transition to more open, lower-biomass forests(1,2,14). Here we present observational evidence for a widespread decline in forest greenness over the past decade based on analyses of satellite data (optical, thermal, microwave and gravity) from several independent sensors over the Congo basin. This decline in vegetation greenness, particularly in the northern Congolese forest, is generally consistent with decreases in rainfall, terrestrial water storage, water content in aboveground woody and leaf biomass, and the canopy backscatter anomaly caused by changes in structure and moisture in upper forest layers. It is also consistent with increases in photosynthetically active radiation and land surface temperature. These multiple lines of evidence indicate that this large-scale vegetation browning, or loss of photosynthetic capacity, may be partially attributable to the long-term drying trend. Our results suggest that a continued gradual decline of photosynthetic capacity and moisture content driven by the persistent drying trend could alter the composition and structure of the Congolese forest to favour the spread of drought-tolerant species(1,2,14).
C1 [Zhou, Liming] SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA.
[Tian, Yuhong] NOAA, IMSG, NESDIS, Ctr Satellite Applicat & Res,STAR, College Pk, MD 20740 USA.
[Myneni, Ranga B.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Ciais, Philippe] UVSQ, CEA, CNRS, LSCE, F-91191 Gif Sur Yvette, France.
[Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Liu, Yi Y.] Univ New S Wales, ARC Ctr Excellence Climate Syst Sci, Sydney, NSW 2052, Australia.
[Liu, Yi Y.] Univ New S Wales, Climate Change Res Ctr, Sydney, NSW 2052, Australia.
[Piao, Shilong] Peking Univ, Dept Ecol, Coll Urban & Environm Sci, Beijing 100871, Peoples R China.
[Chen, Haishan] Nanjing Univ Informat Sci & Technol, Minist Educ, Key Lab Meteorol Disaster, Nanjing 210044, Jiangsu, Peoples R China.
[Vermote, Eric F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Song, Conghe] Univ N Carolina, Dept Geog, Chapel Hill, NC 29599 USA.
[Song, Conghe] Anhui Agr Univ, Sch Forestry & Landscape Architecture, Hefei 230036, Anhui, Peoples R China.
[Hwang, Taehee] Univ N Carolina, Inst Environm, Chapel Hill, NC 29599 USA.
RP Zhou, LM (reprint author), SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA.
EM lzhou@albany.edu
RI Myneni, Ranga/F-5129-2012; Young, Kristina/M-3069-2014; Liu,
Yi/H-9226-2013; Song, Conghe/E-3087-2016; Liu, Yi/M-7169-2015; Zhou,
Liming/A-2688-2012;
OI Song, Conghe/0000-0002-4099-4906; Liu, Yi/0000-0001-9059-8269; Chen,
Haishan/0000-0002-2403-3187
FU NOAA NESDIS [NA11NES4400010]; University at Albany, State University of
New York; NASA's Earth Science Division; National Natural Science
Foundation of China [41230422]
FX This study was supported by the NOAA NESDIS project (NA11NES4400010) and
by the startup funds provided by the University at Albany, State
University of New York. R. B. M. was funded by NASA's Earth Science
Division. The views, opinions, and findings contained in this report are
those of the authors and should not be construed as an official NOAA or
US Government position, policy, or decision. H. C. is supported by the
National Natural Science Foundation of China (grant number 41230422).
NR 51
TC 60
Z9 62
U1 17
U2 249
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD MAY 1
PY 2014
VL 509
IS 7498
BP 86
EP +
DI 10.1038/nature13265
PG 18
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AG1TM
UT WOS:000335199100044
PM 24759324
ER
PT J
AU Oviatt, CG
Chan, MA
Jewell, PW
Bills, BG
Madsen, DB
Miller, DM
AF Oviatt, Charles G.
Chan, Marjorie A.
Jewell, Paul W.
Bills, Bruce G.
Madsen, David B.
Miller, David M.
TI Interpretations of evidence for large Pleistocene paleolakes in the
Bonneville basin, western North America COMMENT on: Bonneville basin
shoreline records of large lake intervals during marine isotope stage 3
and the last glacial maximum, by Nishizawa et al. (2013)
SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY
LA English
DT Article
DE Pleistocene; Great Basin; Radiocarbon; Lake Bonneville; MIS 3
ID UTAH
AB Nishizawa et al. (2013) argue in support of three large paleolakes in the Bonneville basin during Marine Oxygen Isotope Stage 3 (MIS 3). If true, that would be an important contribution to paleoclimate investigations. However, the key evidence in support of their argument consists of four radiocarbon ages that are out of stratigraphic order and near the practical and theoretical limit of the dating method. The interpretation of three large MIS 3 lakes conflicts with some of their own data, as well as with independently derived stratigraphic information from the basin. Nishizawa et al. (2013) also interpret a series of radiocarbon ages of mollusk samples as indicating previously undocumented lake transgressions a few thousand years older than basal radiocarbon ages of wood samples. We believe that these interpretations are in error, and arise largely from reliance on radiocarbon ages from carbonate material. Lake records constrained by ages of non-carbonate organic materials, along with compelling stratigraphic information from unconformities and buried soils, argue for not changing interpretations of Lake Bonneville history until more supporting information for older lakes at relatively high altitudes is found. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Oviatt, Charles G.] Kansas State Univ, Dept Geol, Manhattan, KS 66506 USA.
[Chan, Marjorie A.; Jewell, Paul W.] Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA.
[Bills, Bruce G.] CALTECH, Jet Prop Lab, Asteroids Comets & Satellites Grp, Pasadena, CA 91109 USA.
[Madsen, David B.] Lanzhou Univ, Res Sch Arid Environm & Climate Change, Lanzhou 730000, Peoples R China.
[Miller, David M.] US Geol Survey, Menlo Pk, CA 94025 USA.
RP Oviatt, CG (reprint author), Kansas State Univ, Dept Geol, Manhattan, KS 66506 USA.
EM joviatt@ksu.edu
NR 16
TC 2
Z9 2
U1 0
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0031-0182
EI 1872-616X
J9 PALAEOGEOGR PALAEOCL
JI Paleogeogr. Paleoclimatol. Paleoecol.
PD MAY 1
PY 2014
VL 401
BP 173
EP 176
DI 10.1016/j.palaeo.2014.03.003
PG 4
WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology
SC Physical Geography; Geology; Paleontology
GA AG2YK
UT WOS:000335282800014
ER
PT J
AU Ray, FA
Robinson, E
McKenna, M
Hada, M
George, K
Cucinotta, F
Goodwin, EH
Bedford, JS
Bailey, SM
Cornforth, MN
AF Ray, F. Andrew
Robinson, Erin
McKenna, Miles
Hada, Megumi
George, Kerry
Cucinotta, Francis
Goodwin, Edwin H.
Bedford, Joel S.
Bailey, Susan M.
Cornforth, Michael N.
TI Directional genomic hybridization: inversions as a potential
biodosimeter for retrospective radiation exposure
SO RADIATION AND ENVIRONMENTAL BIOPHYSICS
LA English
DT Article
DE Chromosome inversions; Biodosimetry; Ionizing radiation; FISH; DGH;
Directional genomic hybridization; Strand-specific hybridization
ID IN-SITU HYBRIDIZATION; COMPLEX CHROMOSOME-ABERRATIONS;
IONIZING-RADIATION; HUMAN-LYMPHOCYTES; ALPHA-PARTICLES; GAMMA-RAYS;
HEAVY-IONS; BIOLOGICAL DOSIMETRY; EXCHANGE ABERRATIONS; CYTOGENETIC
METHODS
AB Chromosome aberrations in blood lymphocytes provide a useful measure of past exposure to ionizing radiation. Despite the widespread and successful use of the dicentric assay for retrospective biodosimetry, the approach suffers substantial drawbacks, including the fact that dicentrics in circulating blood have a rather short half-life (roughly 1-2 years by most estimates). So-called symmetrical aberrations such as translocations are far more stable in that regard, but their high background frequency, which increases with age, also makes them less than ideal for biodosimetry. We developed a cytogenetic assay for potential use in retrospective biodosimetry that is based on the detection of chromosomal inversions, another symmetrical aberration whose transmissibility (stability) is also ostensibly high. Many of the well-known difficulties associated with inversion detection were circumvented through the use of directional genomic hybridization, a method of molecular cytogenetics that is less labor intensive and better able to detect small chromosomal inversions than other currently available approaches. Here, we report the dose-dependent induction of inversions following exposure to radiations with vastly different ionization densities [i.e., linear energy transfer (LET)]. Our results show a dramatic dose-dependent difference in the yields of inversions induced by low-LET gamma rays, as compared to more damaging high-LET charged particles similar to those encountered in deep space.
C1 [Ray, F. Andrew; Bedford, Joel S.; Bailey, Susan M.] Colorado State Univ, Dept Environm & Radiol Hlth Sci, Ft Collins, CO 80523 USA.
[Robinson, Erin; McKenna, Miles; Goodwin, Edwin H.] KromaTiD Inc, Ft Collins, CO 80524 USA.
[Hada, Megumi] Univ Space Res Assoc, Houston, TX 77058 USA.
[George, Kerry] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA.
[Cucinotta, Francis] Natl Aeronaut & Space Adm, Houston, TX 77058 USA.
[Cornforth, Michael N.] Univ Texas Med Branch, Dept Radiat Oncol, Galveston, TX 77555 USA.
RP Ray, FA (reprint author), Colorado State Univ, Dept Environm & Radiol Hlth Sci, Ft Collins, CO 80523 USA.
EM fa.ray@colostate.edu
FU NASA [NNX08AB65G, NNX09CE42P, NNX10CB05C, NNJ06HA29A]; NIH/NIAID
[R01AI080486-02]
FX Funding for this work from NASA (NNX08AB65G; NNX09CE42P; NNX10CB05C;
NNJ06HA29A) and NIH/NIAID (R01AI080486-02) is gratefully acknowledged.
NR 49
TC 4
Z9 4
U1 2
U2 9
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0301-634X
EI 1432-2099
J9 RADIAT ENVIRON BIOPH
JI Radiat. Environ. Biophys.
PD MAY
PY 2014
VL 53
IS 2
BP 255
EP 263
DI 10.1007/s00411-014-0513-1
PG 9
WC Biology; Biophysics; Environmental Sciences; Radiology, Nuclear Medicine
& Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Biophysics; Environmental
Sciences & Ecology; Radiology, Nuclear Medicine & Medical Imaging
GA AF8XF
UT WOS:000334998200005
PM 24477407
ER
PT J
AU Pate, DJ
Gray, J
German, BJ
AF Pate, David J.
Gray, Justin
German, Brian J.
TI A graph theoretic approach to problem formulation for multidisciplinary
design analysis and optimization
SO STRUCTURAL AND MULTIDISCIPLINARY OPTIMIZATION
LA English
DT Article
DE Graph theory; Multidisciplinary design optimization; Problem formulation
ID DECOMPOSITION; SYSTEMS
AB The formulation of multidisciplinary design, analysis, and optimization (MDAO) problems has become increasingly complex as the number of analysis tools and design variables included in typical studies has grown. This growth in the scale and scope of MDAO problems has been motivated by the need to incorporate additional disciplines and to expand the parametric design space to enable the exploration of unconventional design concepts. In this context, given a large set of disciplinary analysis tools, the problem of determining a feasible data flow between tools to produce a specified set of system-level outputs is combinatorially challenging. The difficulty is compounded in multi-fidelity problems, which are of increasing interest to the MDAO community. In this paper, we propose an approach for addressing this problem based on the formalism of graph theory. The approach begins by constructing the maximal connectivity graph (MCG) describing all possible interconnections between a set of analysis tools. Graph operations are then conducted to reduce the MCG to a fundamental problem graph (FPG) that describes the connectivity of analysis tools needed to solve a specified system-level design problem. The FPG does not predispose a particular solution procedure; any relevant MDO solution architecture could be selected to implement the optimization. Finally, the solution architecture can be represented in a problem solution graph (PSG). The graph approach is applied to an example problem based on a commercial aircraft MDAO study.
C1 [Pate, David J.; German, Brian J.] Georgia Inst Technol, Sch Aerosp Engn, Atlanta, GA 30332 USA.
[Gray, Justin] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP German, BJ (reprint author), Georgia Inst Technol, Sch Aerosp Engn, 270 Ferst Dr, Atlanta, GA 30332 USA.
EM brian.german@aerospace.gatech.edu
NR 31
TC 0
Z9 0
U1 3
U2 22
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1615-147X
EI 1615-1488
J9 STRUCT MULTIDISCIP O
JI Struct. Multidiscip. Optim.
PD MAY
PY 2014
VL 49
IS 5
BP 743
EP 760
DI 10.1007/s00158-013-1006-6
PG 18
WC Computer Science, Interdisciplinary Applications; Engineering,
Multidisciplinary; Mechanics
SC Computer Science; Engineering; Mechanics
GA AG6EC
UT WOS:000335510400004
ER
PT J
AU Duda, BM
Menter, FR
Hansen, T
Esteve, MJ
Deck, S
Bezard, H
AF Duda, Benjamin M.
Menter, Florian R.
Hansen, Thorsten
Esteve, Marie-Josephe
Deck, Sebastien
Bezard, Herve
TI Aerothermal Prediction of Multiple Hot Jets in Crossflow for Aircraft
Applications
SO AIAA JOURNAL
LA English
DT Article
ID LARGE-EDDY-SIMULATION; SCALE-ADAPTIVE SIMULATION; MODEL
AB Even though many technical applications feature multiple jets in crossflow, little attention has been paid so far to their simultaneous numerical simulation as a system. A special challenge in this context is the simulation of exhausts of air systems on aircraft since they feature multiple hot jets in crossflow at high Reynolds numbers. As standard statistical turbulence models are not capable of correctly predicting thermal mixing between the jet and crossflow as well as interjet mixing, the scale-adaptive simulation is employed. In a first step, a simplified configuration comprising five laterally aligned jets is investigated, and numerical results are compared to wind tunnel data with good agreement. The establishing flowfield is analyzed, and its dynamics are compared to a single jet in the crossflow reference case. In a second step, the exhaust of an existing antiicing system is considered on an aircraft under realistic flight conditions. To take into account the local flow topology and to reduce computational costs, a sequential simulation methodology is applied, which relies on a Reynolds-Averaged Navier-Stokes simulation of the aircraft to provide boundary conditions for a subsequent scale-adaptive simulation calculation in a truncated subdomain. Results are compared to flight test data with good agreement, which highlights the applicability of the proposed approach.
C1 [Duda, Benjamin M.] Airbus Ind, Aerodynam Tools & Simulat, F-31060 Toulouse, France.
[Duda, Benjamin M.] NASA, Langley Res Center, Hampton, VA USA.
[Menter, Florian R.] ANSYS Germany GmbH, Core Dev, D-83624 Otterfing, Germany.
[Hansen, Thorsten] ANSYS Germany GmbH, Customer & Sales Support, D-83624 Otterfing, Germany.
[Esteve, Marie-Josephe] Airbus Ind, Aerodynam Tools & Simulat, F-31060 Toulouse, France.
[Deck, Sebastien] Off Natl Etud & Rech Aerosp, Appl Aerodynam Dept, F-92190 Meudon, France.
[Bezard, Herve] Off Natl Etud & Rech Aerosp, Aerodynam & Energet Modeling Dept, F-31055 Toulouse, France.
RP Duda, BM (reprint author), Airbus Ind, Aerodynam Tools & Simulat, F-31060 Toulouse, France.
OI Deck, Sebastien/0000-0003-1020-0965
NR 28
TC 0
Z9 1
U1 1
U2 8
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 MAY
PY 2014
VL 52
IS 5
BP 1035
EP 1046
DI 10.2514/1.J052370
PG 12
WC Engineering, Aerospace
SC Engineering
GA AF7AE
UT WOS:000334864900012
ER
PT J
AU Bregon, A
Daigle, M
Roychoudhury, I
Biswas, G
Koutsoukos, X
Pulido, B
AF Bregon, Anibal
Daigle, Matthew
Roychoudhury, Indranil
Biswas, Gautam
Koutsoukos, Xenofon
Pulido, Belarmino
TI An event-based distributed diagnosis framework using structural model
decomposition
SO ARTIFICIAL INTELLIGENCE
LA English
DT Article
DE Distributed diagnosis; Structural model decomposition; Discrete event
systems; Possible Conflicts
ID ANALYTICAL REDUNDANCY RELATIONS; FAULT-DIAGNOSIS; FAILURE DIAGNOSIS;
SYSTEMS; DIAGNOSABILITY; ALGORITHM; CONFLICTS; NETWORKS
AB Complex engineering systems require efficient on-line fault diagnosis methodologies to improve safety and reduce maintenance costs. Traditionally, diagnosis approaches are centralized, but these solutions do not scale well. Also, centralized diagnosis solutions are difficult to implement on increasingly prevalent distributed, networked embedded systems. This paper presents a distributed diagnosis framework for physical systems with continuous behavior. Using Possible Conflicts, a structural model decomposition method from the Artificial Intelligence model-based diagnosis (DX) community, we develop a distributed diagnoser design algorithm to build local event-based diagnosers. These diagnosers are constructed based on global diagnosability analysis of the system, enabling them to generate local diagnosis results that are globally correct without the use of a centralized coordinator. We also use Possible Conflicts to design local parameter estimators that are integrated with the local diagnosers to form a comprehensive distributed diagnosis framework. Hence, this is a fully distributed approach to fault detection, isolation, and identification. We evaluate the developed scheme on a four-wheeled rover for different design scenarios to show the advantages of using Possible Conflicts, and generate on-line diagnosis results in simulation to demonstrate the approach. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Bregon, Anibal; Pulido, Belarmino] Univ Valladolid, Dept Comp Sci, E-47011 Valladolid, Spain.
[Daigle, Matthew] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Roychoudhury, Indranil] NASA, Ames Res Ctr, SGT Inc, Moffett Field, CA 94035 USA.
[Biswas, Gautam; Koutsoukos, Xenofon] Vanderbilt Univ, Dept Elect Engn & Comp Sci, Inst Software Integrated Syst, Nashville, TN 37235 USA.
RP Bregon, A (reprint author), Univ Valladolid, Dept Comp Sci, E-47011 Valladolid, Spain.
EM anibal@infor.uva.es; matthew.j.daigle@nasa.gov;
indranil.roychoudhury@nasa.gov; gautam.biswas@vanderbilt.edu;
xenofon.koutsoukos@vanderbilt.edu; belar@infor.uva.es
RI Pulido Junquera, Belarmino/I-2506-2015;
OI Pulido Junquera, Belarmino/0000-0003-2340-684X; Daigle,
Matthew/0000-0002-4616-3302
FU Spanish MCI grant [TIN2009-11326]; NASA System-wide Safety and Assurance
Technologies (SSAT) project; National Science Foundation [CNS-1238959]
FX A. Bregon and B. Pulido's work has been partially supported by the
Spanish MCI TIN2009-11326 grant.; M. Daigle and I. Roychoudhury's work
has been partially supported by the NASA System-wide Safety and
Assurance Technologies (SSAT) project.; Xenofon Koutsoukos' work was
supported in part by the National Science Foundation (CNS-1238959).
NR 58
TC 8
Z9 8
U1 0
U2 21
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0004-3702
EI 1872-7921
J9 ARTIF INTELL
JI Artif. Intell.
PD MAY
PY 2014
VL 210
BP 1
EP 35
DI 10.1016/j.artint.2014.01.003
PG 35
WC Computer Science, Artificial Intelligence
SC Computer Science
GA AF8OF
UT WOS:000334974800001
ER
PT J
AU Coughlin, JL
Thompson, SE
Bryson, ST
Burke, CJ
Caldwell, DA
Christiansen, JL
Haas, MR
Howell, SB
Jenkins, JM
Kolodziejczak, JJ
Mullally, FR
Rowe, JF
AF Coughlin, Jeffrey L.
Thompson, Susan E.
Bryson, Stephen T.
Burke, Christopher J.
Caldwell, Douglas A.
Christiansen, Jessie L.
Haas, Michael R.
Howell, Steve B.
Jenkins, Jon M.
Kolodziejczak, Jeffery J.
Mullally, Fergal R.
Rowe, Jason F.
TI CONTAMINATION IN THE KEPLER FIELD. IDENTIFICATION OF 685 KOIs AS FALSE
POSITIVES VIA EPHEMERIS MATCHING BASED ON Q1-Q12 DATA
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; instrumentation: detectors; planetary systems;
planets and satellites: detection; stars: statistics; techniques:
photometric
ID ECLIPSING BINARIES; PLANET HUNTERS; DATA RELEASE; VALIDATION; CATALOG;
SYSTEMS
AB The Kepler mission has to date found almost 6000 planetary transit-like signals, utilizing three years of data for over 170,000 stars at extremely high photometric precision. Due to its design, contamination from eclipsing binaries, variable stars, and other transiting planets results in a significant number of these signals being false positives (FPs). This directly affects the determination of the occurrence rate of Earth-like planets in our Galaxy, as well as other planet population statistics. In order to detect as many of these FPs as possible, we perform ephemeris matching among all transiting planet, eclipsing binary, and variable star sources. We find that 685 Kepler Objects of Interest (KOIs)-12% of all those analyzed-are FPs as a result of contamination, due to 409 unique parent sources. Of these, 118 have not previously been identified by other methods. We estimate that similar to 35% of KOIs are FPs due to contamination, when performing a first-order correction for observational bias. Comparing single-planet candidate KOIs to multi-planet candidate KOIs, we find an observed FP fraction due to contamination of 16% and 2.4% respectively, bolstering the existing evidence that multi-planet KOIs are significantly less likely to be FPs. We also analyze the parameter distributions of the ephemeris matches and derive a simple model for the most common type of contamination in the Kepler field. We find that the ephemeris matching technique is able to identify low signal-to-noise FPs that are difficult to identify with other vetting techniques. We expect FP KOIs to become more frequent when analyzing more quarters of Kepler data, and note that many of them will not be able to be identified based on Kepler data alone.
C1 [Coughlin, Jeffrey L.; Thompson, Susan E.; Burke, Christopher J.; Caldwell, Douglas A.; Jenkins, Jon M.; Mullally, Fergal R.; Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA.
[Coughlin, Jeffrey L.; Thompson, Susan E.; Bryson, Stephen T.; Burke, Christopher J.; Caldwell, Douglas A.; Haas, Michael R.; Howell, Steve B.; Jenkins, Jon M.; Mullally, Fergal R.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Christiansen, Jessie L.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Kolodziejczak, Jeffery J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Coughlin, JL (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM jeffrey.l.coughlin@nasa.gov
RI Caldwell, Douglas/L-7911-2014
OI Caldwell, Douglas/0000-0003-1963-9616
FU NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; NASA
Science Mission directorate
FX We thank the anonymous referee for his or her very helpful comments,
which especially helped to improve the clarity of the paper. 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. This research has made use of NASA's Astrophysics
Data System. Some of the data presented in this paper were obtained from
the Mikulski Archive for Space Telescopes (MAST). STScI is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS5-26555. Support for MAST for non-HST data is provided
by the NASA Office of Space Science via grant NNX09AF08G and by other
grants and contracts. This paper includes data collected by the Kepler
mission. Funding for the Kepler mission is provided by the NASA Science
Mission directorate.
NR 24
TC 32
Z9 32
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD MAY
PY 2014
VL 147
IS 5
AR 119
DI 10.1088/0004-6256/147/5/119
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF3DO
UT WOS:000334591900026
ER
PT J
AU O'Dea, JA
Jenet, FA
Cheng, TH
Buu, CM
Beroiz, M
Asmar, SW
Armstrong, JW
AF O'Dea, J. Andrew
Jenet, F. A.
Cheng, Tsan-Huei
Buu, Chau M.
Beroiz, Martin
Asmar, Sami W.
Armstrong, J. W.
TI BRIGHT MICROWAVE PULSES FROM PSR B0531+21 OBSERVED WITH A PROTOTYPE
TRANSIENT SURVEY RECEIVER
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE instrumentation: detectors; pulsars: individual (B0531+21)
ID ANISOTROPIC MAGNETOGASDYNAMIC TURBULENCE; CRAB PULSAR;
INTERSTELLAR-MEDIUM; DENSITY-FLUCTUATIONS; RADIO TRANSIENT; GIANT
PULSES; SCINTILLATION; SCATTERING; EMISSION; SPECTRUM
AB Recent discoveries of transient radio events have renewed interest in time-variable astrophysical phenomena. Many radio transient events are rare, requiring long observing times for reliable statistical study. The National Aeronautics and Space Administration/Jet Propulsion Laboratory's Deep Space Network (DSN) tracks spacecraft nearly continuously with 13 large-aperture, low system temperature radio antennas. During normal spacecraft operations, the DSN processes only a small fraction of the pre-detection bandwidth available from these antennas; any information in the remaining bandwidth, e.g., from an astronomical source in the same antenna beam as the spacecraft, is currently ignored. As a firmware modification to the standard DSN tracking receiver, we built a prototype receiver that could be used for astronomical transient surveys. Here, we demonstrate the receiver's utility through observations of bright pulses from the Crab pulsar and describe attributes of potential transient survey observations piggybacking on operational DSN tracks.
C1 [O'Dea, J. Andrew; Cheng, Tsan-Huei; Buu, Chau M.; Asmar, Sami W.; Armstrong, J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Jenet, F. A.; Beroiz, Martin] Univ Texas Brownsville, Dept Phys & Astron, Brownsville, TX 78520 USA.
RP O'Dea, JA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
FU JPL; National Aeronautics and Space Administration
FX The authors thank Ron Creech and Larry Bracamonte of ITT and the
Goldstone team for supporting the test passes at DSS15. We benefited
from discussions with W. A. Coles and Richard Woo. Development of the
RRAT TRAP prototype was supported under the Director's Research and
Development Fund at JPL. For the JPL authors, the research described
here was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 31
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD MAY
PY 2014
VL 147
IS 5
AR 100
DI 10.1088/0004-6256/147/5/100
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF3DO
UT WOS:000334591900007
ER
PT J
AU Kourdis, PD
Bellan, J
AF Kourdis, Panayotis D.
Bellan, Josette
TI Heavy-alkane oxidation kinetic-mechanism reduction using dominant
dynamic variables, self similarity and chemistry tabulation
SO COMBUSTION AND FLAME
LA English
DT Article
DE Reduced kinetics for n-heptane; Iso-octane; n-Decane and n-dodecane;
Self-similarity; Dominant variable
ID EQUATION-OF-STATE; SENSITIVITY FUNCTIONS; COMBUSTION; MODELS; JET
AB A model of local and full or partial self similarity is developed for situations in which a phenomenon exhibits a dominant variable, with the goal of applying the model to obtain reduced oxidation kinetics from detailed kinetics for n-heptane, iso-octane, n-decane and n-dodecane. Upon appropriate normalization, it is shown that the state vector for all four alkanes indeed obeys local full self similarity with respect to the dominant variable which is here a normalized temperature. Further, the vector of species mass fractions is partitioned into major species which are those of interest to calculate, and thus for which equations are solved, and minor species which are those of no interest to calculate and are therefore modeled. The goal of the chemical kinetic reduction is to provide a model which expresses the influence of the minor species on the major species. The identification of major species with the light species, and of the minor species with the heavy species leads to partitioning the energetics into computed and modeled parts. This partition of the species set is shown to lead to local full self similarity of the reaction rates between the modeled and calculated species; the local full self similarity also prevails for the energy of the modeled species and for the average heat capacity at constant volume of the heavy species. A methodology is developed to take advantage of this self similarity by considering the initial condition as a point in the three-dimensional space of the initial pressure, initial temperature and equivalence ratio, choosing eight points surrounding the initial condition in this space, developing the self similarity graphs at these eight points using the LLNL detailed mechanism in conjunction with CHEMKIN II, and calculating at each time step the modeled contributions at the surrounded point by interpolating from those known at the eight points. Once the modeled contributions are known, the conservation equations for the species and the energy, coupled with a real-gas equation of state, are solved. With a focus on the high-pressure conditions in automotive engines, extensive results are shown for the four alkanes over a wide range of initial temperatures (650-1000 K) and equivalence ratios (0.35-3.00) at 20 bar and 40 bar. The results consist of timewise profiles of the temperature and species, allowing the calculation of the ignition time and the equilibrium or maximum temperature. Comparisons between the reduced mechanism and the detailed mechanism show excellent to very good agreement for all alkanes when only 20 progress-variable light species are used in the reduced mechanism; the 20 species are the same for all fuels, and for n-decane and n-dodecane this represents a reduction in the species progress variables by factor of more than 100. As an example, calculations that excellently duplicate the elemental mechanism are also shown for n-dodecane using only 15 or 6 progress-variable light species, indicating the potential for further progress-variable reduction beyond the 20 species. (C) 2013 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Kourdis, Panayotis D.; Bellan, Josette] CALTECH, Pasadena, CA 91125 USA.
[Bellan, Josette] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bellan, J (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM Josette.Bellan@jpl.nasa.gov
FU Army Research Office
FX This study was conducted at the California Institute of Technology, Jet
Propulsion Laboratory (JPL), and was sponsored by the Army Research
Office, with Dr. Ralph Anthenien as Program Manager. Interesting
discussions with, as well as suggestions and information from Dr.
Kenneth G. Harstad are gratefully acknowledged. Computations were
performed using the JPL/NASA Supercomputing facilities.
NR 15
TC 2
Z9 2
U1 7
U2 22
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0010-2180
EI 1556-2921
J9 COMBUST FLAME
JI Combust. Flame
PD MAY
PY 2014
VL 161
IS 5
BP 1196
EP 1223
DI 10.1016/j.combustflame.2013.11.012
PG 28
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA AF4AO
UT WOS:000334654000006
ER
PT J
AU Tonui, E
Zolensky, M
Hiroi, T
Nakamura, T
Lipschutz, ME
Wang, MS
Okudaira, K
AF Tonui, Eric
Zolensky, Mike
Hiroi, Takahiro
Nakamura, Tomoki
Lipschutz, Michael E.
Wang, Ming-Sheng
Okudaira, Kyoko
TI Petrographic, chemical and spectroscopic evidence for thermal
metamorphism in carbonaceous chondrites I: CI and CM chondrites (vol
126, pg 284, 2014)
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Correction
C1 [Tonui, Eric] BP Upstream Res & Technol, Houston, TX 77079 USA.
[Zolensky, Mike] NASA, Johnson Space Ctr, ARES, Houston, TX 77058 USA.
[Hiroi, Takahiro] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Nakamura, Tomoki] Tohoku Univ Aramaki, Dept Earth & Planetary Mat Sci, Fac Sci, Sendai, Miyagi 9808578, Japan.
[Lipschutz, Michael E.; Wang, Ming-Sheng] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA.
[Okudaira, Kyoko] Univ Aizu, Aizu Wakamatsu, Fukushima 9658580, Japan.
RP Tonui, E (reprint author), BP Upstream Res & Technol, 501 Westlake Blvd, Houston, TX 77079 USA.
NR 1
TC 0
Z9 0
U1 1
U2 2
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 MAY 1
PY 2014
VL 132
BP 458
EP 458
DI 10.1016/j.gca.2014.02.022
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AF6NP
UT WOS:000334832100025
ER
PT J
AU Olsen, N
Luhr, H
Finlay, CC
Sabaka, TJ
Michaelis, I
Rauberg, J
Toffner-Clausen, L
AF Olsen, Nils
Luehr, Hermann
Finlay, Christopher C.
Sabaka, Terence J.
Michaelis, Ingo
Rauberg, Jan
Toffner-Clausen, Lars
TI The CHAOS-4 geomagnetic field model
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Inverse theory; Magnetic anomalies: modelling and interpretation; Rapid
time variations; Satellite magnetics
ID EARTHS MAGNETIC-FIELD; SECULAR VARIATION; OBSERVATORY DATA; SATELLITE
DATA; POLAR VORTEX; CORE; CHAMP
AB We present CHAOS-4, a new version in the CHAOS model series, which aims to describe the Earth's magnetic field with high spatial and temporal resolution. Terms up to spherical degree of at least n = 85 for the lithospheric field, and up to n = 16 for the time-varying core field are robustly determined.
More than 14 yr of data from the satellites circle divide rsted, CHAMP and SAC-C, augmented with magnetic observatory monthly mean values have been used for this model. Maximum spherical harmonic degree of the static (lithospheric) field is n = 100. The core field is expressed by spherical harmonic expansion coefficients up to n = 20; its time-evolution is described by order six splines, with 6-month knot spacing, spanning the time interval 1997.0-2013.5. The third time derivative of the squared radial magnetic field component is regularized at the core-mantle boundary. No spatial regularization is applied to the core field, but the high-degree lithospheric field is regularized for n > 85.
CHAOS-4 model is derived by merging two submodels: its low-degree part has been derived using similar model parametrization and data sets as used for previous CHAOS models (but of course including more recent data), while its high-degree lithospheric field part is solely determined from low-altitude CHAMP satellite observations taken during the last 2 yr (2008 September-2010 September) of the mission. We obtain a good agreement with other recent lithospheric field models like MF7 for degrees up to n = 85, confirming that lithospheric field structures down to a horizontal wavelength of 500 km are currently robustly determined.
C1 [Olsen, Nils; Finlay, Christopher C.; Toffner-Clausen, Lars] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Luehr, Hermann; Michaelis, Ingo; Rauberg, Jan] Deutsch GeoForschungsZentrum GFZ, Helmholtz Zentrum Potsdam, D-14473 Potsdam, Germany.
[Sabaka, Terence J.] NASA, Goddard Space Flight Ctr, Geodynam Branch, Greenbelt, MD 20771 USA.
RP Olsen, N (reprint author), Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JW, Midlothian, Scotland.
RI Finlay, Christopher/B-5062-2014; Olsen, Nils/H-1822-2011;
OI Finlay, Christopher/0000-0002-4592-2290; Olsen,
Nils/0000-0003-1132-6113; Toffner-Clausen, Lars/0000-0003-4314-3776
FU CHAMP mission by the German Aerospace Center (DLR); Federal Ministry of
Education and Research
FX This paper has been finalised while N.O. was visiting Professor at
University of Edinburgh, kindly supported by The Leverhulme Trust. We
would like to thank the staff of the geomagnetic observatories and
INTERMAGNET for supplying high-quality observatory data, and Susan
Macmillan for providing us with checked and corrected observatory hourly
mean values. The support of the CHAMP mission by the German Aerospace
Center (DLR) and the Federal Ministry of Education and Research is
gratefully acknowledged. The Orsted Project was made possible by
extensive support from the Danish Government, NASA, ESA, CNES, DARA and
the Thomas B. Thriges Foundation.
NR 49
TC 52
Z9 54
U1 1
U2 19
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0956-540X
EI 1365-246X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD MAY
PY 2014
VL 197
IS 2
BP 815
EP 827
DI 10.1093/gji/ggu033
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AF5EK
UT WOS:000334736600010
ER
PT J
AU Casner, SM
Schooler, JW
AF Casner, Stephen M.
Schooler, Jonathan W.
TI Thoughts in Flight Automation Use and Pilots' Task-Related and
Task-Unrelated Thought
SO HUMAN FACTORS
LA English
DT Article
DE awareness; mind wandering; attention; cockpit automation
ID TIME-ESTIMATION; MIND; PERFORMANCE
AB Objective:
The objective was to examine the relationship between cockpit automation use and task-related and task-unrelated thought among airline pilots.
Background:
Studies find that cockpit automation can sometimes relieve pilots of tedious control tasks and afford them more time to think ahead. Paradoxically, automation has also been shown to lead to lesser awareness. These results prompt the question of what pilots think about while using automation.
Method:
A total of 18 airline pilots flew a Boeing 747-400 simulator while we recorded which of two levels of automation they used. As they worked, pilots were verbally probed about what they were thinking. Pilots were asked to categorize their thoughts as pertaining to (a) a specific task at hand, (b) higher-level flight-related thoughts (e.g., planning ahead), or (c) thoughts unrelated to the flight. Pilots' performance was also measured.
Results:
Pilots reported a smaller percentage of task-at-hand thoughts (27% vs. 50%) and a greater percentage of higher-level flight-related thoughts (56% vs. 29%) when using the higher level of automation. However, when all was going according to plan, using either level of automation, pilots also reported a higher percentage of task-unrelated thoughts (21%) than they did when in the midst of an unsuccessful performance (7%). Task-unrelated thoughts peaked at 25% when pilots were not interacting with the automation.
Conclusion:
Although cockpit automation may provide pilots with more time to think, it may encourage pilots to reinvest only some of this mental free time in thinking flight-related thoughts.
Application:
This research informs the design of human-automation systems that more meaningfully engage the human operator.
C1 [Casner, Stephen M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Schooler, Jonathan W.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA.
RP Casner, SM (reprint author), NASA, Ames Res Ctr, Mail Stop 262-4, Moffett Field, CA 94035 USA.
EM stephen.casner@nasa.gov
FU Aviation Safety Program at the National Aeronautics and Space
Administration
FX This work was supported by the Aviation Safety Program at the National
Aeronautics and Space Administration.
NR 27
TC 7
Z9 7
U1 1
U2 16
PU SAGE PUBLICATIONS INC
PI THOUSAND OAKS
PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA
SN 0018-7208
EI 1547-8181
J9 HUM FACTORS
JI Hum. Factors
PD MAY
PY 2014
VL 56
IS 3
BP 433
EP 442
DI 10.1177/0018720813501550
PG 10
WC Behavioral Sciences; Engineering, Industrial; Ergonomics; Psychology,
Applied; Psychology
SC Behavioral Sciences; Engineering; Psychology
GA AF3SJ
UT WOS:000334632200001
PM 24930166
ER
PT J
AU Davis, CA
Ahijevych, DA
Haggerty, JA
Mahoney, MJ
AF Davis, Christopher A.
Ahijevych, David A.
Haggerty, Julie A.
Mahoney, Michael J.
TI Observations of Temperature in the Upper Troposphere and Lower
Stratosphere of Tropical Weather Disturbances
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Tropopause; Aircraft observations; Microwave observations; Convective
clouds; Tropical cyclones
ID TROPOPAUSE REGION; CLOUDS; WAVES; CONVECTION; EVOLUTION; ATLANTIC;
CLIMATE; PREDICT; LAYER; CYCLOGENESIS
AB Microwave temperature profiler (MTP) data are analyzed to document temperature signatures in the upper troposphere and lower stratosphere that accompany Atlantic tropical weather disturbances. The MTP was deployed on the National Science Foundation-National Center for Atmospheric Research Gulfstream V (GV) aircraft during the Pre-Depression Investigation of Cloud-Systems in the Tropics (PREDICT) in August and September 2010.
Temporal variations in cold-point temperature compared with infrared cloud-top temperature reveal that organized deep convection penetrated to near or beyond the cold point for each of the four disturbances that developed into a tropical cyclone. Relative to the lower-tropospheric circulation center, MTP and dropsonde data confirmed a stronger negative radial gradient of temperature in the upper troposphere (10-13 km) of developing disturbances prior to genesis compared with nondeveloping disturbances. The MTP data revealed a somewhat higher and shallower area of relative warmth near the center when compared with dropsonde data. MTP profiles through anvil cloud depicted cooling near 15 km and warming in the lower stratosphere near the time of maximum coverage of anvil clouds shortly after sunrise. Warming occurred through a deep layer of the upper troposphere toward local noon, presumably associated with radiative heating in cloud. The temperature signatures of anvil cloud above 10-km altitude contributed to the radial gradient of temperature because of the clustering of deep convection near the center of circulation. However, it is concluded that these signatures may be more a result of properties of convection than a direct distinguishing factor of genesis.
C1 [Davis, Christopher A.; Ahijevych, David A.; Haggerty, Julie A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Mahoney, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Davis, CA (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
EM cdavis@ucar.edu
FU National Science Foundation
FX The National Center for Atmospheric Research is sponsored by the
National Science Foundation.
NR 50
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U1 2
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD MAY
PY 2014
VL 71
IS 5
BP 1593
EP 1608
DI 10.1175/JAS-D-13-0278.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF8UQ
UT WOS:000334991500005
ER
PT J
AU Shen, BW
AF Shen, Bo-Wen
TI Nonlinear Feedback in a Five-Dimensional Lorenz Model
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Differential equations; Nonlinear dynamics; Numerical weather
prediction/forecasting; Climate prediction; Lyapunov vectors; Numerical
analysis/modeling
ID GENERAL-CIRCULATION MODEL; LOCAL LYAPUNOV EXPONENTS; OCEAN-ATMOSPHERE
MODEL; BENARD CONVECTION; TIME-SERIES; PREDICTABILITY; TRUNCATIONS;
ORDER; CHAOS; SYSTEMS
AB In this study, based on the number of modes, the original three-dimensional Lorenz model (3DLM) is generalized with two additional modes [five-dimensional Lorenz model (5DLM)] to examine their role in the predictability of the numerical solutions and to understand the underlying processes that increase the solution stability. As a result of the simplicity of the 5DLM with respect to existing generalized Lorenz models (LMs), the author is able to obtain the analytical solutions of its critical points and identify the role of the major nonlinear term in the solution's stability, which have previously not been documented in the literature. The nonlinear Jacobian terms of the governing equations are analyzed to highlight the importance of selecting new modes for extending the nonlinear feedback loop of the 3DLM and thus effectively increasing the degree of nonlinearity (i.e., the nonlinear mode-mode interactions) in the 5DLM. It is then shown that numerical solutions in the 5DLM require a larger normalized Rayleigh number r for the onset of chaos and are more predictable than those in the 3DLM when r is between 25 and 40 and the Prandtl number sigma is 10. The improved predictability is attributable to the negative nonlinear feedback enabled by the new modes. The role of the (negative) nonlinear feedback is further verified using a revised 3DLM with a parameterized nonlinear eddy dissipative term. The finding of the increased stability in the 5DLM and revised 3DLM with respect to the 3DLM is confirmed with the linear stability analysis and the analysis of the Lyapunov exponents using different values of r and sigma. To further understand the impact of an additional heating term, results from the 5DLM and a higher-dimensional LM [e.g., the six-dimensional LM (6DLM)] are analyzed and compared.
C1 [Shen, Bo-Wen] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Shen, Bo-Wen] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Shen, BW (reprint author), NASA, Mesoscale Atmospher Proc Lab, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM bo-wen.shen-1@nasa.gov
FU NASA Advanced Information System Technology (AIST) program of the Earth
Science Technology Office (ESTO); NASA Computational Modeling Algorithms
and Cyberinfrastructure (CMAC) program
FX We thank anonymous reviewers, Drs. Y.-L. Lin, R. Anthes, X. Zeng, R.
Pielke, J. Dutton, A. Molod, H.-M. H. Juang, S. Cheung, C.-L. Shie, and
Y.-L. Wu for their valuable comments and encouragement, Professor Z. Wu
for providing the code for the calculation of Gaussian white noise, and
Ms. J. Dunbar and K. Massaro for proofreading this manuscript. We are
grateful for support from the NASA Advanced Information System
Technology (AIST) program of the Earth Science Technology Office (ESTO)
and from the NASA Computational Modeling Algorithms and
Cyberinfrastructure (CMAC) program. Resources supporting this work were
provided by the NASA High-End Computing (HEC) program through the NASA
Advanced Supercomputing division at Ames Research Center. Special thanks
are due to the library personnel of NASA GSFC Library for helping obtain
a copy of several classical journal articles.
NR 42
TC 7
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U1 0
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD MAY
PY 2014
VL 71
IS 5
BP 1701
EP 1723
DI 10.1175/JAS-D-13-0223.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF8UQ
UT WOS:000334991500011
ER
PT J
AU Chung, D
Matheou, G
AF Chung, Daniel
Matheou, Georgios
TI Large-Eddy Simulation of Stratified Turbulence. Part I: A Vortex-Based
Subgrid-Scale Model
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Large eddy simulations; Subgrid-scale processes
ID PLANETARY BOUNDARY-LAYER; STRETCHED SPIRAL VORTICES; ATMOSPHERIC
SURFACE-LAYER; ISOTROPIC TURBULENCE; CHANNEL FLOW; NUMERICAL-SIMULATION;
CUMULUS CONVECTION; ENERGY-DISSIPATION; STRESS MODEL; VELOCITY
AB The stretched-vortex subgrid-scale (SGS) model is extended to enable large-eddy simulation of buoyancy-stratified turbulence. Both stable and unstable stratifications are considered. The extended model retains the anisotropic form of the original stretched-vortex model, but the SGS kinetic energy and the characteristic SGS eddy size are modified by buoyancy subject to two constraints: first, the SGS kinetic energy dynamics is determined by stationary and homogeneous conditions, and second, the SGS eddy size obeys a scaling analogous to the Monin-Obukhov similarity theory. The SGS model construction, comprising an ensemble of subgrid stretched-vortical structures, naturally limits vertical mixing but allows horizontal mixing provided the alignment of the SGS vortex ensemble is favorable, even at high nominal gradient Richardson numbers. In very stable stratification, the model recovers the z-less limit, in which a vortex-based Obukhov length controls the SGS dynamics, while in very unstable stratification, the model recovers the free-convection limit, in which a vortex-based Deardorff velocity controls the SGS dynamics. The efficacy of the present SGS model is demonstrated by simulating the canonical stationary and homogeneous, stratified sheared turbulence at high Reynolds numbers and moderately high Richardson numbers. In the postprocessing, the SGS dynamics of the stretched-vortex model is further interrogated to yield predictions of buoyancy-adjusted one-dimensional SGS spectra and SGS root-mean-square velocity-derivative fluctuations.
C1 [Chung, Daniel] Univ Melbourne, Dept Mech Engn, Melbourne, Vic 3010, Australia.
[Matheou, Georgios] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Chung, D (reprint author), Univ Melbourne, Dept Mech Engn, Melbourne, Vic 3010, Australia.
EM daniel.chung@unimelb.edu.au
RI Chung, Daniel/F-4468-2016
OI Chung, Daniel/0000-0003-3732-364X
FU Office of Naval Research, Marine Meteorology Program [N0001411IP20087,
N0001411IP20069]; NASA MAP Program; NOAA/CPO MAPP Program; National
Aeronautics and Space Administration
FX 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. We 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. 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 69
TC 11
Z9 11
U1 0
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD MAY
PY 2014
VL 71
IS 5
BP 1863
EP 1879
DI 10.1175/JAS-D-13-0126.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF8UQ
UT WOS:000334991500019
ER
PT J
AU Johansen, CT
Mcrae, CD
Danehy, PM
Gallo, ECA
Cantu, LML
Magnotti, G
Cutler, AD
Rockwell, RD
Goyne, CP
McDaniel, JC
AF Johansen, Craig T.
McRae, Colin D.
Danehy, Paul M.
Gallo, Emanuela C. A.
Cantu, Luca M. L.
Magnotti, Gaetano
Cutler, Andrew D.
Rockwell, Robert D., Jr.
Goyne, Chris P.
McDaniel, James C.
TI OH PLIF visualization of the UVa supersonic combustion experiment:
configuration A
SO JOURNAL OF VISUALIZATION
LA English
DT Article
DE Flow visualization; Planar laser-induced fluorescence; Supersonic
combustion
ID SCRAMJET ENGINES; TUNNEL
AB Hydroxyl radical (OH) planar laser-induced fluorescence (PLIF) visualizations were performed in the University of Virginia supersonic combustion experiment. The test section was set up in configuration A, which includes a Mach 2 nozzle, combustor, and extender section. Hydrogen fuel was injected through an unswept compression ramp at two different equivalence ratios. Through the translation of the optical system and the use of two separate camera views, the entire optically accessible range of the combustor was imaged. Single-shot, average, and standard deviation images of the OH PLIF signal are presented at several streamwise locations. The results show the development of a highly turbulent flame structure and provide an experimental database to be used for numerical model assessment.
C1 [Johansen, Craig T.; McRae, Colin D.] Univ Calgary, Calgary, AB, Canada.
[Danehy, Paul M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Gallo, Emanuela C. A.; Cantu, Luca M. L.; Magnotti, Gaetano; Cutler, Andrew D.] George Washington Univ, Newport News, VA USA.
[Rockwell, Robert D., Jr.; Goyne, Chris P.; McDaniel, James C.] Univ Virginia, Charlottesville, VA USA.
RP Mcrae, CD (reprint author), Univ Calgary, Calgary, AB, Canada.
EM johansen@ucalgary.ca; mcraec@ucalgary.ca
OI Magnotti, Gaetano/0000-0002-1723-5258
FU Natural Sciences and Engineering Research Council of Canada (NSERC); Air
Force Office of Scientific Research (AFOSR); NASA National Center for
Hypersonic Combined Cycle Propulsion [FA 9550-09-1-0611]
FX Dr. Johansen was supported by the Natural Sciences and Engineering
Research Council of Canada (NSERC). This work was supported by the Air
Force Office of Scientific Research (AFOSR) and NASA National Center for
Hypersonic Combined Cycle Propulsion grant FA 9550-09-1-0611. The
technical monitors are Chiping Li from the AFOSR and Rick Gaffney from
NASA.
NR 22
TC 6
Z9 6
U1 3
U2 20
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1343-8875
EI 1875-8975
J9 J VISUAL-JAPAN
JI J. Vis.
PD MAY
PY 2014
VL 17
IS 2
BP 131
EP 141
DI 10.1007/s12650-014-0197-2
PG 11
WC Computer Science, Interdisciplinary Applications; Imaging Science &
Photographic Technology
SC Computer Science; Imaging Science & Photographic Technology
GA AF1XJ
UT WOS:000334506900005
ER
PT J
AU Clarke, GB
Wilson, EL
Miller, JH
Melroy, HR
AF Clarke, G. B.
Wilson, E. L.
Miller, J. H.
Melroy, H. R.
TI Uncertainty analysis for the miniaturized laser heterodyne radiometer
(mini-LHR) for the measurement of carbon dioxide in the atmospheric
column
SO MEASUREMENT SCIENCE AND TECHNOLOGY
LA English
DT Article
DE laser heterodyne radiometer; carbon dioxide ( CO2); radio frequency (
RF) receiver; column abundance; remote sensing
ID AERONET
AB Presented here is a sensitivity analysis for the miniaturized laser heterodyne radiometer. This passive, ground-based instrument measures carbon dioxide (CO2) in the atmospheric column and has been under development at NASA/ GSFC since 2009. The goal of this development is to produce a low-cost, easily-deployable instrument that can extend current ground measurement networks in order to (1) validate column satellite observations, (2) provide coverage in regions of limited satellite observations, (3) target regions of interest such as thawing permafrost, and (4) support the continuity of a long-term climate record. In this paper an uncertainty analysis of the instrument performance is presented and compared with results from three sets of field measurements. The signal-to-noise ratio (SNR) and corresponding maximum uncertainty for a single scan are calculated to be 329.4 +/- 1.3 by deploying error propagation through the equation governing the SNR. Reported is an absorbance noise of 0.0024 for six averaged scans of field data, for an instrument precision of 0.14 ppmv for CO2.
C1 [Clarke, G. B.] Amer Univ, Washington, DC 20016 USA.
[Clarke, G. B.; Wilson, E. L.; Melroy, H. R.] NASA, Goddard Space Flight Ctr, Laser Remote Sensing Lab, Greenbelt, MD 20771 USA.
[Miller, J. H.; Melroy, H. R.] George Washington Univ, Dept Chem, Washington, DC 20052 USA.
RP Clarke, GB (reprint author), Amer Univ, 4400 Massachusetts Ave, Washington, DC 20016 USA.
EM gclarke@american.edu
NR 14
TC 2
Z9 2
U1 3
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-0233
EI 1361-6501
J9 MEAS SCI TECHNOL
JI Meas. Sci. Technol.
PD MAY
PY 2014
VL 25
IS 5
AR 055204
DI 10.1088/0957-0233/25/5/055204
PG 5
WC Engineering, Multidisciplinary; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA AE9TD
UT WOS:000334352000022
ER
PT J
AU Lane, WM
Cotton, WD
van Velzen, S
Clarke, TE
Kassim, NE
Helmboldt, JF
Lazio, TJW
Cohen, AS
AF Lane, W. M.
Cotton, W. D.
van Velzen, S.
Clarke, T. E.
Kassim, N. E.
Helmboldt, J. F.
Lazio, T. J. W.
Cohen, A. S.
TI The Very Large Array Low-frequency Sky Survey Redux (VLSSr)
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: image processing; catalogues; surveys; radio continuum:
general
ID STAR-FORMATION HISTORY; RADIO-SOURCES; SOURCE CATALOG; SPECTRUM;
EVOLUTION; GALAXIES; UNIVERSE; SCALE; AREA
AB We present the results of a recent re-reduction of the data from the Very Large Array (VLA) Low-frequency Sky Survey (VLSS). We used the VLSS catalogue as a sky model to correct the ionospheric distortions in the data and create a new set of sky maps and corresponding catalogue at 73.8 MHz. The VLSS Redux (VLSSr) has a resolution of 75 arcsec, and an average map rms noise level of Sigma similar to 0.1 Jy beam(-1). The clean bias is 0.66 x Sigma and the theoretical largest angular size is 36 arcmin. Six previously unimaged fields are included in the VLSSr, which has an unbroken sky coverage over 9.3 sr above an irregular southern boundary. The final catalogue includes 92 964 sources. The VLSSr improves upon the original VLSS in a number of areas including imaging of large sources, image sensitivity, and clean bias; however the most critical improvement is the replacement of an inaccurate primary beam correction which caused source flux errors which vary as a function of radius to nearest pointing centre in the VLSS.
C1 [Lane, W. M.; Clarke, T. E.; Kassim, N. E.; Helmboldt, J. F.] Naval Res Lab, Washington, DC 20375 USA.
[Cotton, W. D.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[van Velzen, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cohen, A. S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Lane, WM (reprint author), Naval Res Lab, Code 7213,4555 Overlook Ave SW, Washington, DC 20375 USA.
EM wendy.peters@nrl.navy.mil
RI Helmboldt, Joseph/C-8105-2012
FU 6.1 base funds; National Aeronautics and Space Administration
FX Basic research at the Naval Research Lab is supported by 6.1 base funds.
We thank E. Polisensky for help with the graphics. Part of this research
was carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration. The National Radio Astronomy Observatory is a facility
of the National Science Foundation operated under cooperative agreement
by Associated Universities, Inc.
NR 42
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U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2014
VL 440
IS 1
BP 327
EP 338
DI 10.1093/mnras/stu256
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF4OD
UT WOS:000334691900026
ER
PT J
AU Negrello, M
Hopwood, R
Dye, S
da Cunha, E
Serjeant, S
Fritz, J
Rowlands, K
Fleuren, S
Bussmann, RS
Cooray, A
Dannerbauer, H
Gonzalez-Nuevo, J
Lapi, A
Omont, A
Amber, S
Auld, R
Baes, M
Buttiglione, S
Cava, A
Danese, L
Dariush, A
De Zotti, G
Dunne, L
Eales, S
Ibar, E
Ivison, RJ
Kim, S
Leeuw, L
Maddox, S
Michalowski, MJ
Massardi, M
Pascale, E
Pohlen, M
Rigby, E
Smith, DJB
Sutherland, W
Temi, P
Wardlow, J
AF Negrello, M.
Hopwood, R.
Dye, S.
da Cunha, E.
Serjeant, S.
Fritz, J.
Rowlands, K.
Fleuren, S.
Bussmann, R. S.
Cooray, A.
Dannerbauer, H.
Gonzalez-Nuevo, J.
Lapi, A.
Omont, A.
Amber, S.
Auld, R.
Baes, M.
Buttiglione, S.
Cava, A.
Danese, L.
Dariush, A.
De Zotti, G.
Dunne, L.
Eales, S.
Ibar, E.
Ivison, R. J.
Kim, S.
Leeuw, L.
Maddox, S.
Michalowski, M. J.
Massardi, M.
Pascale, E.
Pohlen, M.
Rigby, E.
Smith, D. J. B.
Sutherland, W.
Temi, P.
Wardlow, J.
TI Herschel-ATLAS: deep HST/WFC3 imaging of strongly lensed submillimetre
galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: strong; galaxies: elliptical and lenticular, cD;
galaxies: evolution; galaxies: formation; infrared: galaxies;
submillimetre: galaxies
ID SCIENCE DEMONSTRATION PHASE; EXTRAGALACTIC SURVEY; LUMINOSITY FUNCTIONS;
INFRARED-EMISSION; HIGH-REDSHIFT; SIMPLE-MODEL; BLACK-HOLES; DUST;
EVOLUTION; STELLAR
AB We report on deep near-infrared observations obtained with the Wide Field Camera-3 (WFC3) onboard the Hubble Space Telescope (HST) of the first five confirmed gravitational lensing events discovered by the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). We succeed in disentangling the background galaxy from the lens to gain separate photometry of the two components. The HST data allow us to significantly improve on previous constraints of the mass in stars of the lensed galaxy and to perform accurate lens modelling of these systems, as described in the accompanying paper by Dye et al. We fit the spectral energy distributions of the background sources from near-IR to millimetre wavelengths and use the magnification factors estimated by Dye et al. to derive the intrinsic properties of the lensed galaxies. We find these galaxies to have star-formations rates (SFR) similar to 400-2000 M-circle dot yr(-1), with similar to(6-25) x 10(10) M-circle dot of their baryonic mass already turned into stars. At these rates of star formation, all remaining molecular gas will be exhausted in less than similar to 100 Myr, reaching a final mass in stars of a few 10(11) M-circle dot. These galaxies are thus proto-ellipticals caught during their major episode of star formation, and observed at the peak epoch (z similar to 1.5-3) of the cosmic star formation history of the Universe.
C1 [Negrello, M.; Buttiglione, S.; De Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England.
[Dye, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[da Cunha, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Serjeant, S.; Amber, S.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Fritz, J.; Baes, M.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Rowlands, K.] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Fleuren, S.; Sutherland, W.] Univ London, Sch Math Sci, London E1 4NS, England.
[Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bussmann, R. S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Cooray, A.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Dannerbauer, H.] Univ Vienna, Inst Astron, A-1160 Vienna, Austria.
[Gonzalez-Nuevo, J.] Inst Fis Cantabria CSIC UC, E-39005 Santander, Spain.
[Lapi, A.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Lapi, A.; Danese, L.; De Zotti, G.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Omont, A.] Univ Paris 06, UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
[Omont, A.] CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
[Auld, R.; Dariush, A.; Eales, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Cava, A.] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland.
[Dunne, L.; Maddox, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Ibar, E.] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile.
[Ivison, R. J.] European So Observ, D-85748 Garching, Germany.
[Ivison, R. J.; Michalowski, M. J.] Univ Edinburgh, Inst Astron, Scottish Univ Phys Alliance, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Kim, S.] Catholic Univ Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Leeuw, L.] UNISA, Coll Grad Studies, ZA-0003 Unisa, South Africa.
[Massardi, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy.
[Rigby, E.] Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Smith, D. J. B.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
RP Negrello, M (reprint author), Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy.
EM mattia.negrello@oapd.inaf.it
RI Wardlow, Julie/C-9903-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; Ivison,
R./G-4450-2011; Cava, Antonio/C-5274-2017;
OI Baes, Maarten/0000-0002-3930-2757; Maddox, Stephen/0000-0001-5549-195X;
Dye, Simon/0000-0002-1318-8343; Wardlow, Julie/0000-0003-2376-8971;
Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Smith,
Daniel/0000-0001-9708-253X; Ivison, R./0000-0001-5118-1313; Cava,
Antonio/0000-0002-4821-1275; De Zotti, Gianfranco/0000-0003-2868-2595
FU STFC [PP/D002400/1, ST/G002533/1]; ASI/INAF [I/072/09/0]; PRIN-INAF;
Spanish Ministerio de Ciencia e Innovacion [AYA2010-21766-C03-01];
Spanish CSIC; European Social Fund; National Aeronautics and Space
Administration
FX This work was supported by STFC (grants PP/D002400/1 and ST/G002533/1),
by ASI/INAF agreement I/072/09/0, by PRIN-INAF 2012 project 'Looking
into the dust-obscured phase of galaxy formation through cosmic zoom
lenses in the Herschel Astrophysical Large Area Survey' and, in part, by
the Spanish Ministerio de Ciencia e Innovacion (project
AYA2010-21766-C03-01). JGN acknowledges financial support from the
Spanish CSIC for a JAE-DOC fellowship, co-funded by the European Social
Fund. Herschel is an ESA space observatory with science instruments
provided by European-led Principal Investigator consortia and with
important participation from NASA. The Herschel-ATLAS is a project with
Herschel, which is an ESA space observatory with science instruments
provided by European-led Principal Investigator consortia and with
important participation from NASA. The H-ATLAS website is
http://www.h-atlas.org/. This publication makes use of data products
from the WISE, 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 61
TC 26
Z9 26
U1 0
U2 15
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 MAY
PY 2014
VL 440
IS 3
BP 1999
EP 2012
DI 10.1093/mnras/stu413
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF5HG
UT WOS:000334744000009
ER
PT J
AU Marinucci, A
Matt, G
Kara, E
Miniutti, G
Elvis, M
Arevalo, P
Ballantyne, DR
Balokovic, M
Bauer, F
Brenneman, L
Boggs, SE
Cappi, M
Christensen, FE
Craig, WW
Fabian, AC
Fuerst, F
Hailey, CJ
Harrison, FA
Risaliti, G
Reynolds, CS
Stern, DK
Walton, DJ
Zhang, W
AF Marinucci, A.
Matt, G.
Kara, E.
Miniutti, G.
Elvis, M.
Arevalo, P.
Ballantyne, D. R.
Balokovic, M.
Bauer, F.
Brenneman, L.
Boggs, S. E.
Cappi, M.
Christensen, F. E.
Craig, W. W.
Fabian, A. C.
Fuerst, F.
Hailey, C. J.
Harrison, F. A.
Risaliti, G.
Reynolds, C. S.
Stern, D. K.
Walton, D. J.
Zhang, W.
TI Simultaneous NuSTAR and XMM-Newton 0.5-80 keV spectroscopy of the
narrow-line Seyfert 1 galaxy SWIFT J2127.4+5654
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; galaxies: active; galaxies: individual:
SWIFT J2127.4+5654; galaxies: Seyfert
ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; HIGH-ENERGY OBSERVATIONS;
PHOTON IMAGING CAMERA; RAY-EMITTING REGION; X-RAY; IRON K; BEPPOSAX
OBSERVATIONS; REVERBERATION LAGS; COSMIC EVOLUTION
AB We present a broad-band spectral analysis of the joint XMM-Newton and Nuclear Spectroscopic Telescope Array observational campaign of the narrow-line Seyfert 1 SWIFT J2127.4+5654, consisting of 300 ks performed during three XMM-Newton orbits. We detect a relativistic broadened iron K alpha line originating from the innermost regions of the accretion disc surrounding the central black hole, from which we infer an intermediate spin of a = 0.58(-0.17)(+0.11). The intrinsic spectrum is steep (Gamma = 2.08 +/- 0.01) as commonly found in narrow-line Seyfert 1 galaxies, while the cutoff energy (Ec = 108(-10)(+11)kev) falls within the range observed in broad-line Seyfert 1 galaxies. We measure a low-frequency lag that increases steadily with energy, while at high frequencies, there is a clear lag following the shape of the broad Fe K emission line. Interestingly, the observed Fe K lag in SWIFT J2127.4+5654 is not as broad as in other sources that have maximally spinning black holes. The lag amplitude suggests a continuum-to-reprocessor distance of about 10-20 r(g). These timing results independently support an intermediate black hole spin and a compact corona.
C1 [Marinucci, A.; Matt, G.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy.
[Kara, E.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England.
[Miniutti, G.] Ctr Astrobiol CSIC INTA, Dep Astrofis, E-28691 Madrid, Spain.
[Miniutti, G.] ESAC, E-28691 Madrid, Spain.
[Elvis, M.; Brenneman, L.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Arevalo, P.; Bauer, F.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 22, Chile.
[Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Balokovic, M.; Fuerst, F.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Cappi, M.] IASF Bologna, INAF, I-40129 Bologna, Italy.
[Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Stern, D. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Marinucci, A (reprint author), Univ Roma Tre, Dipartimento Fis, Via Vasca Navale 84, I-00146 Rome, Italy.
EM marinucci@fis.uniroma3.it
RI Miniutti, Giovanni/L-2721-2014; Boggs, Steven/E-4170-2015; Cappi,
Massimo/F-4813-2015;
OI Miniutti, Giovanni/0000-0003-0707-4531; Boggs,
Steven/0000-0001-9567-4224; Cappi, Massimo/0000-0001-6966-8920;
Risaliti, Guido/0000-0002-3556-977X
FU Italian Space Agency [ASI/INAFI/037/12/0-011/13]; European Union
[312789]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024];
Anillo ACT1101; International Fulbright Science and Technology Award;
NASA [NNG08FD60C]; National Aeronautics and Space Administration
FX We thank the referee for her/his comments and suggestions that greatly
improved the paper. AM thanks Javier Garcia and Thomas Dauser for the
efforts in producing XILLVER and RELXILL tables to use in this paper. AM
and GM acknowledge financial support from Italian Space Agency under
grant ASI/INAFI/037/12/0-011/13 and from the European Union Seventh
Framework Programme (FP7/2007-2013) under grant agreement no. 312789. PA
and FB acknowledge support from Basal-CATA PFB-06/2007 (FEB),
CONICYT-Chile FONDECYT 1101024 (FEB) and Anillo ACT1101 (FEB, PA). MB
acknowledges support from the International Fulbright Science and
Technology Award. 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).
NR 69
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U1 1
U2 5
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2014
VL 440
IS 3
BP 2347
EP 2356
DI 10.1093/mnras/stu404
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF5HG
UT WOS:000334744000033
ER
PT J
AU Schultz, MR
Rose, CA
Guzman, JC
McCarville, D
Hilburger, MW
AF Schultz, Marc R.
Rose, Cheryl A.
Guzman, J. Carlos
McCarville, Douglas
Hilburger, Mark W.
TI An experimental study of the compression response of fluted-core
composite panels with joints
SO COMPOSITES PART B-ENGINEERING
LA English
DT Article
DE Polymer matrix composites (PMCs); Mechanical testing; Joints/joining;
Fluted-core sandwich composites
AB Fluted-core sandwich composites consist of integral angled web members spaced between laminate facesheets, and may have the potential to provide benefits over traditional sandwich composites for certain aerospace applications. However, fabrication of large autoclave-cured fluted-core cylindrical shells with existing autoclaves will require that the shells be fabricated in segments, and joined longitudinally to form a complete barrel. Experiments on two different fluted-core longitudinal joint designs were considered in this study. In particular, jointed fluted-core-composite panels were tested in longitudinal compression because this is the primary loading condition in dry launch-vehicle barrel sections. One of the joint designs performed well in comparison with unjointed test articles, and the other joint design failed at loads approximately 14% lower than unjointed test articles. The compression-after-impact (CAI) performance of jointed fluted-core composites was also investigated with test articles that had been subjected to 6 ft-lb impacts from a 1/2-in, hemispherical indenter. It was found that such impacts reduced the load-carrying capability by 9 similar to 40%. This reduction was dependent on the joint concept. (C) 2014 Published by Elsevier Ltd.
C1 [Schultz, Marc R.; Rose, Cheryl A.; Hilburger, Mark W.] NASA, Struct Mech & Concepts Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Guzman, J. Carlos; McCarville, Douglas] Boeing Co, Boeing Res & Technol, Seattle, WA 98124 USA.
RP Schultz, MR (reprint author), NASA, Struct Mech & Concepts Branch, Langley Res Ctr, Mail Stop 190, Hampton, VA 23681 USA.
EM marc.r.schultz@nasa.gov
FU NASA Engineering and Safety Center (NESC) Shell Buckling Knockdown
Factor Project, NESC [07-010-E]
FX This work was conducted as part of the NASA Engineering and Safety
Center (NESC) Shell Buckling Knockdown Factor Project, NESC assessment
number 07-010-E. All of the panels used to make the test articles
discussed herein were produced and provided by The Boeing Company.
Jeffrey Seebo of Analytical Mechanics Associates, Inc. at NASA Langley
developed the system used for the ultrasonic scans and was instrumental
in interpreting the data. The ultrasonic scans were performed by Richard
Churray of NASA Langley.
NR 7
TC 0
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U1 0
U2 0
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1359-8368
EI 1879-1069
J9 COMPOS PART B-ENG
JI Compos. Pt. B-Eng.
PD MAY
PY 2014
VL 61
BP 229
EP 237
DI 10.1016/j.compositesb.2013.12.029
PG 9
WC Engineering, Multidisciplinary; Materials Science, Composites
SC Engineering; Materials Science
GA AE6UQ
UT WOS:000334133900027
ER
PT J
AU Burow, LC
Woebken, D
Marshall, IPG
Singer, SW
Pett-Ridge, J
Prufert-Bebout, L
Spormann, AM
Bebout, BM
Weber, PK
Hoehler, TM
AF Burow, L. C.
Woebken, D.
Marshall, I. P. G.
Singer, S. W.
Pett-Ridge, J.
Prufert-Bebout, L.
Spormann, A. M.
Bebout, B. M.
Weber, P. K.
Hoehler, T. M.
TI Identification of Desulfobacterales as primary hydrogenotrophs in a
complex microbial mat community
SO GEOBIOLOGY
LA English
DT Article
ID SULFATE-REDUCING BACTERIA; SP-NOV; GEN. NOV.; DIVERSITY; SEDIMENTS;
ECOLOGY; BIOGEOCHEMISTRY; METHANOGENESIS; SEQUENCES; REDUCTION
AB Hypersaline microbial mats have been shown to produce significant quantities of H-2 under dark, anoxic conditions via cyanobacterial fermentation. This flux of a widely accessible microbial substrate has potential to significantly influence the ecology of the mat, and any consumption will affect the net efflux of H-2 that might otherwise be captured as a resource. Here, we focus on H-2 consumption in a microbial mat from Elkhorn Slough, California, USA, for which H-2 production has been previously characterized. Active biologic H-2 consumption in this mat is indicated by a significant time-dependent decrease in added H-2 compared with a killed control. Inhibition of sulfate reduction, as indicated by a decrease in hydrogen sulfide production relative to controls, resulted in a significant increase in H-2 efflux, suggesting that sulfate-reducing bacteria (SRB) are important hydrogenotrophs. Low methane efflux under these same conditions indicated that methanogens are likely not important hydrogenotrophs. Analyses of genes and transcripts that encode for rRNA or dissimilatory sulfite reductase, using both PCR-dependent and PCR-independent metatranscriptomic sequencing methods, demonstrated that Desulfobacterales are the dominant, active SRB in the upper, H-2-producing layer of the mat (0-2mm). This hypothesis was further supported by the identification of transcripts encoding hydrogenases derived from Desulfobacterales capable of H-2 oxidation. Analysis of molecular data provided no evidence for the activity of hydrogenotrophic methanogens. The combined biogeochemical and molecular data strongly indicate that SRB belonging to the Desulfobacterales are the quantitatively important hydrogenotrophs in the Elkhorn Slough mat.
C1 [Burow, L. C.; Woebken, D.; Marshall, I. P. G.; Spormann, A. M.] Stanford Univ, Dept Chem Engn, Stanford, CA 94305 USA.
[Burow, L. C.; Woebken, D.; Marshall, I. P. G.; Spormann, A. M.] Stanford Univ, Dept Civil Engn, Stanford, CA 94305 USA.
[Burow, L. C.; Woebken, D.; Marshall, I. P. G.; Spormann, A. M.] Stanford Univ, Dept Environm Engn, Stanford, CA 94305 USA.
[Burow, L. C.; Woebken, D.; Prufert-Bebout, L.; Bebout, B. M.; Hoehler, T. M.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Singer, S. W.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94720 USA.
[Pett-Ridge, J.; Weber, P. K.] Lawrence Livermore Natl Lab, Div Chem Sci, Livermore, CA USA.
RP Burow, LC (reprint author), IP Australia, Appl Chem & Biotechnol Sect, Dept Ind, Canberra, ACT, Australia.
EM tori.m.hoehler@nasa.gov; tori.m.hoehler@nasa.gov
RI Woebken, Dagmar/A-4447-2013;
OI Woebken, Dagmar/0000-0002-1314-9926
FU US Department of Energy at Lawrence Livermore National Laboratory
[DE-AC52-07NA27344]; US Department of Energy at Lawrence Berkeley
National Laboratory [DE-AC02-05CH11231]; Office of Science of the U.S.
Department of Energy [DE-AC02-05CH11231]; German Research Foundation
(Deutsche Forschungsgemeinschaft); US. Department of Energy (DOE)
Genomic Science Program [SCW1039]
FX We thank Angela Detweiler and Adrienne Frisbee at the NASA Ames Research
Center for technical support and Tijana Glavina del Rio, Susannah
Tringe, Erika Lindquist and Stephanie Malfatti at the Joint Genome
Institute for assistance obtaining rRNA pyrotag and metatranscriptomic
sequences. We thank Jeff Cann, Associate Wildlife Biologist, Central
Region, California Department of Fish and Game for coordinating our
access to the Elkhorn Slough Wildlife Area. Work at LLNL was performed
under the auspices of the US Department of Energy at Lawrence Livermore
National Laboratory under Contract DE-AC52-07NA27344. Work at LBNL was
performed under the auspices of the US Department of Energy at Lawrence
Berkeley National Laboratory under Contract DE-AC02-05CH11231. Pyrotag
and metatranscriptomic sequencing were conducted by the Joint Genome
Institute, which is supported by the Office of Science of the U.S.
Department of Energy under Contract No. DE-AC02-05CH11231. DW was
partially funded by the German Research Foundation (Deutsche
Forschungsgemeinschaft). Funding was provided by the US. Department of
Energy (DOE) Genomic Science Program under contract SCW1039.
NR 47
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Z9 8
U1 6
U2 35
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1472-4677
EI 1472-4669
J9 GEOBIOLOGY
JI Geobiology
PD MAY
PY 2014
VL 12
IS 3
BP 221
EP 230
DI 10.1111/gbi.12080
PG 10
WC Biology; Environmental Sciences; Geosciences, Multidisciplinary
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Geology
GA AE9WI
UT WOS:000334361800004
PM 24730641
ER
PT J
AU Russell, JA
Brady, AL
Cardman, Z
Slater, GF
Lim, DSS
Biddle, JF
AF Russell, J. A.
Brady, A. L.
Cardman, Z.
Slater, G. F.
Lim, D. S. S.
Biddle, J. F.
TI Prokaryote populations of extant microbialites along a depth gradient in
Pavilion Lake, British Columbia, Canada
SO GEOBIOLOGY
LA English
DT Article
ID MODERN MARINE STROMATOLITES; FRESH-WATER MICROBIALITES; CANDIDATUS
CHLORACIDOBACTERIUM THERMOPHILUM; LITHIFIED MICRITIC LAMINAE;
SULFATE-REDUCING BACTERIA; DRY VALLEY LAKES; CUATRO CIENEGAS; SHARK BAY;
COMPARATIVE METAGENOMICS; WESTERN-AUSTRALIA
AB Pavilion Lake in British Columbia, Canada, is home to modern-day microbialites that are actively growing at multiple depths within the lake. While microbialite morphology changes with depth and previous isotopic investigations suggested a biological role in the formation of these carbonate structures, little is known about their microbial communities. Microbialite samples acquired through the Pavilion Lake Research Project (PLRP) were first investigated for phototrophic populations using Cyanobacteria-specific primers and 16S rRNA gene cloning. These data were expounded on by high-throughput tagged sequencing analyses of the general bacteria population. These molecular analyses show that the microbial communities of Pavilion Lake microbialites are diverse compared to non-lithifying microbial mats also found in the lake. Phototrophs and heterotrophs were detected, including species from the recently described Chloroacidobacteria genus, a photoheterotroph that has not been previously observed in microbialite systems. Phototrophs were shown as the most influential contributors to community differences above and below 25 meters, and corresponding shifts in heterotrophic populations were observed at this interface as well. The isotopic composition of carbonate also mirrored this shift in community states. Comparisons to previous studies indicated this population shift may be a consequence of changes in lake chemistry at this depth. Microbial community composition did not correlate with changing microbialite morphology with depth, suggesting something other than community changes may be a key to observed variations in microbialite structure.
C1 [Russell, J. A.; Biddle, J. F.] Univ Delaware, Sch Marine Sci & Policy, Lewes, DE 19958 USA.
[Brady, A. L.] Univ Calgary, Dept Biol Sci, Calgary, AB T2N 1N4, Canada.
[Cardman, Z.] Univ N Carolina, Chapel Hill, NC USA.
[Slater, G. F.] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON, Canada.
[Lim, D. S. S.] NASA Ames Res Ctr, Moffett Field, CA USA.
[Lim, D. S. S.] SETI Inst, Mountain View, CA USA.
RP Biddle, JF (reprint author), Univ Calgary, Dept Biol Sci, 2500 Univ Dr 1 NW, Calgary, AB T2N 1N4, Canada.
EM jfbiddle@udel.edu
RI Biddle, Jennifer/F-8323-2010;
OI Biddle, Jennifer/0000-0002-4344-8724; Russell,
Joseph/0000-0002-0623-5519
FU NASA Moon and Mars Analog Mission Activities (MMAMA) grant; Canadian
Space Agency's (CSA) Canadian Analogue Research Network (CARN); Analogue
Missions programs, Nuytco Research, the Delaware Space Grant Consortium;
NASA CAN [NNX10AN63H]; Marian R. Okie Fellowship; National Science
Foundation EPSCoR Grant [EPS-0814251]; State of Delaware
FX Special thanks to Donnie Reid and all members of the PLRP field team,
especially the science divers and deep worker pilots who collected the
samples. We thank Jennifer Hansen for laboratory assistance with
carbonate measurements. This work was supported by the NASA Moon and
Mars Analog Mission Activities (MMAMA) grant to D. Lim, the Canadian
Space Agency's (CSA) Canadian Analogue Research Network (CARN), and
Analogue Missions programs, Nuytco Research, the Delaware Space Grant
Consortium funded by NASA CAN NNX10AN63H to D. Mullan and by the UD
College of Earth, Ocean, and Environment. J. Russell was supported by a
Marian R. Okie Fellowship. This publication was made possible by the
National Science Foundation EPSCoR Grant No. EPS-0814251 and the State
of Delaware. We are also grateful to Linda and Mickey Macri for hosting
the PLRP project from 2004 to present and to the Ts'Kw'aylaxw First
Nation and British Columbia Parks for their continued support of our
research. This is Pavilion Lake Research Project publication # 13-02.
NR 63
TC 7
Z9 7
U1 0
U2 23
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1472-4677
EI 1472-4669
J9 GEOBIOLOGY
JI Geobiology
PD MAY
PY 2014
VL 12
IS 3
BP 250
EP 264
DI 10.1111/gbi.12082
PG 15
WC Biology; Environmental Sciences; Geosciences, Multidisciplinary
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Geology
GA AE9WI
UT WOS:000334361800006
PM 24636451
ER
PT J
AU Benafan, O
Noebe, RD
Padula, SA
Brown, DW
Vogel, S
Vaidyanathan, R
AF Benafan, O.
Noebe, R. D.
Padula, S. A., II
Brown, D. W.
Vogel, S.
Vaidyanathan, R.
TI Thermomechanical cycling of a NiTi shape memory alloy-macroscopic
response and microstructural evolution
SO INTERNATIONAL JOURNAL OF PLASTICITY
LA English
DT Article
DE Phase transformation; Microstructures; Twinning; Polycrystalline
material; Mechanical testing
ID REVERSIBLE MARTENSITIC-TRANSFORMATION; LOW-TEMPERATURE CREEP; TI-NI;
TEXTURE ANALYSIS; NEUTRON-DIFFRACTION; ELECTRICAL-RESISTIVITY;
PHASE-TRANSFORMATIONS; CONSTITUTIVE MODEL; BINARY NITI; R-PHASE
AB Thermomechanical cycling of a Ni49.9Ti50.1 (at.%) shape memory alloy was investigated. Combined ex situ macroscopic experiments and in situ neutron diffraction measurements were performed to relate the macroscopic evolution in behavior (e.g., dimensional instabilities) observed during thermal cycling to the responsible microscopic mechanism(s) through texture, internal strain, peak shape, and phase evolution from the neutron data. Pre-deformation in the austenite or martensite phases affected the macroscopic cyclic behavior (e.g., actuation strain), depending on the level of pre-strain and the associated microstructural changes. However, the pre-deformation did not completely stabilize the cyclic response. Subsequent thermomechanical cycling revealed that the martensite texture changed with continued thermal cycling, while the austenite texture did not. For the conditions investigated, stagnation of the martensite texture occurred around the eighth cycle, consistent with asymptotic saturation of the macroscopic transformation strains. Moreover, diffraction spectra peak shapes (broadening) were found to vary with cycling indicative of the accumulation of lattice defects, consistent with the constant increase in residual strain. Published by Elsevier Ltd.
C1 [Benafan, O.; Vaidyanathan, R.] Univ Cent Florida, Adv Mat Proc & Anal Ctr, Mech Mat & Aerosp Engn Dept, Orlando, FL 32816 USA.
[Benafan, O.; Noebe, R. D.; Padula, S. A., II] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Brown, D. W.; Vogel, S.] Los Alamos Natl Lab, Lujan Ctr, Los Alamos, NM 87545 USA.
RP Benafan, O (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
EM othmane.benafan@nasa.gov
OI Vogel, Sven C./0000-0003-2049-0361
FU NASA Fundamental Aeronautics Program, Aeronautical Sciences Project;
Office of Basic Energy Sciences DOE; DOE [DE-AC52-06NA25396];
[NNX08AB51A]
FX Funding from the NASA Fundamental Aeronautics Program, Aeronautical
Sciences Project is gratefully acknowledged. Grant NNX08AB51A to UCF is
gratefully acknowledged. The authors thank B. Clausen, T. Sisneros and
M. Helmut at LANL and D. Gaydosh, A. Garg and G. Bigelow at NASA GRC for
technical support and helpful discussions. D.E. Nicholson's help in
performing the neutron diffraction experiments is gratefully
acknowledged. This work has benefited from the use of the Lujan Neutron
Scattering Center at LANSCE, which is funded by the Office of Basic
Energy Sciences DOE. LANL is operated by Los Alamos National Security
LLC under DOE Contract No. DE-AC52-06NA25396.
NR 89
TC 20
Z9 21
U1 4
U2 41
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0749-6419
EI 1879-2154
J9 INT J PLASTICITY
JI Int. J. Plast.
PD MAY
PY 2014
VL 56
BP 99
EP 118
DI 10.1016/j.ijplas.2014.01.006
PG 20
WC Engineering, Mechanical; Materials Science, Multidisciplinary; Mechanics
SC Engineering; Materials Science; Mechanics
GA AE6EI
UT WOS:000334083000005
ER
PT J
AU Goldberg, RK
Binienda, WK
AF Goldberg, Robert K.
Binienda, Wieslaw K.
TI Special Section on Advances in Ballistic Impact and Crashworthiness
Response of Aerospace Structures
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Editorial Material
C1 [Goldberg, Robert K.] NASA, Res Aerosp Engn, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
RP Goldberg, RK (reprint author), NASA, Res Aerosp Engn, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Robert.K.Goldberg@nasa.gov; wbinienda@uakron.edu
NR 0
TC 0
Z9 0
U1 2
U2 18
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
EI 1943-5525
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD MAY 1
PY 2014
VL 27
IS 3
BP 423
EP 423
DI 10.1061/(ASCE)AS.1943-5525.0000414
PG 1
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA AE9RU
UT WOS:000334347400001
ER
PT J
AU Jackson, KE
Fasanella, EL
Polanco, MA
AF Jackson, K. E.
Fasanella, E. L.
Polanco, M. A.
TI Simulating the Response of a Composite Honeycomb Energy Absorber. I:
Dynamic Crushing of Components and Multiterrain Impacts
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE LS-DYNA; Composite materials; Structural impact; Multiterrain impact;
Explicit simulation; Energy absorption; Crushing
ID FUSELAGE SECTION
AB This paper describes the experimental and analytical evaluation of an externally deployable composite honeycomb structure that is designed to attenuate impact energy during helicopter crashes. The concept, designated the deployable energy absorber (DEA), uses an expandable Kevlar honeycomb to dissipate kinetic energy through crushing. The DEA incorporates a unique flexible-hinge design that enables the honeycomb to be packaged and stowed efficiently until needed for deployment. Experimental evaluation of the DEA included dynamic crush tests of multicell components and vertical drop tests of a composite fuselage section retrofitted with DEA blocks onto multiterrain. Finite-element models of the test articles were developed and simulations were performed using the transient dynamic code LS-DYNA. In each simulation, the DEA was represented using shell elements assigned two different material properties: Mat 24, an isotropic piecewise linear plasticity model, and Mat 58, a continuum damage mechanics model used to represent laminated composite fabrics. DEA model development and test analysis comparisons are presented.
C1 [Jackson, K. E.] NASA, Struct Dynam Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Fasanella, E. L.] NASA, Natl Inst Aerosp, Langley Res Ctr, Hampton, VA 23681 USA.
[Polanco, M. A.] Eagle Technol LLC, Hampton, VA 23666 USA.
RP Jackson, KE (reprint author), NASA, Struct Dynam Branch, Langley Res Ctr, 12 West Bush Rd, Hampton, VA 23681 USA.
EM karen.e.jackson-1@nasa.gov; edwin.l.fasanella@nasa.gov;
mpolanco@eagleaviationtech.com
NR 31
TC 1
Z9 1
U1 4
U2 31
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
EI 1943-5525
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD MAY 1
PY 2014
VL 27
IS 3
BP 424
EP 436
DI 10.1061/(ASCE)AS.1943-5525.0000357
PG 13
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA AE9RU
UT WOS:000334347400002
ER
PT J
AU Fasanella, EL
Annett, MS
Jackson, KE
Polanco, MA
AF Fasanella, E. L.
Annett, M. S.
Jackson, K. E.
Polanco, M. A.
TI Simulating the Response of a Composite Honeycomb Energy Absorber. II:
Full-Scale Impact Testing
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Explicit transient dynamic finite-element simulation; Energy absorption;
Composite materials; Full-scale crash testing
AB The National Aeronautics and Space Administration (NASA) has sponsored research to evaluate an externally deployable composite honeycomb designed to attenuate loads in the event of a helicopter crash. The concept, designated the deployable energy absorber (DEA), is an expandable Kevlar honeycomb. The DEA incorporates a flexible hinge that allows the honeycomb to be stowed collapsed until needed during an emergency. Evaluation of the DEA began with material characterization of the Kevlar-129 fabric/epoxy and ended with a full-scale crash test of a retrofitted MD-500 helicopter. During each evaluation phase, finite-element (FE) models of the test articles were developed, and simulations were performed using the dynamic FE code LS-DYNA. This paper focuses on simulations of two full-scale impact tests involving the DEA: a mass simulator and a DEA-retrofitted MD-500 helicopter. Isotropic (Mat 24) and composite (Mat 58) material models that were assigned to DEA shell elements were compared. Based on simulation results, the Mat 58 model showed better agreement with the test results.
C1 [Fasanella, E. L.] NASA, Natl Inst Aerosp, Langley Res Ctr, Hampton, VA 23681 USA.
[Annett, M. S.] NASA, Struct Dynam Branch, Langley Res Ctr, Hampton, VA USA.
[Jackson, K. E.] NASA, Struct Dynam Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Polanco, M. A.] Eagle Technol LLC, Hampton, VA 23666 USA.
RP Fasanella, EL (reprint author), NASA, Natl Inst Aerosp, Langley Res Ctr, 12 West Bush Rd, Hampton, VA 23681 USA.
EM edwin.l.fasanella@nasa.gov; martin.s.annett@nasa.gov;
karen.e.jackson-1@nasa.gov; mpolanco@eagleaviationtech.com
NR 20
TC 2
Z9 2
U1 0
U2 17
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
EI 1943-5525
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD MAY 1
PY 2014
VL 27
IS 3
BP 437
EP 441
DI 10.1061/(ASCE)AS.1943-5525.0000358
PG 5
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA AE9RU
UT WOS:000334347400003
ER
PT J
AU Vassilakos, GJ
Hardy, RC
AF Vassilakos, Gregory J.
Hardy, Robin C.
TI Sand Impact Tests of a Half-Scale Crew Module Test Article
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Sand (material); Simulation models; Spacecraft; Impact tests
AB Although the Orion Multi-Purpose Crew Vehicle (MPCV) is being designed primarily for water landings, the possibility exists of an onshore landing at Kennedy Space Center (KSC) following a launch abort. To obtain data to evaluate the adequacy of sand material models used in beach landing simulations, sand impact tests were conducted at National Aeronautics and Space Administration (NASA) Langley Research Center (LRC). Both vertical drop tests and swing tests with combined vertical and horizontal velocity were performed onto beds of common construction-grade sand using a geometrically scaled crew module test article. The tests were simulated using the explicit, nonlinear, transient dynamic finite-element code LS-DYNA. The shape of the test article was similar to a scaled crew module, but the structure was much heavier and was sufficiently robust to survive multiple impacts without permanent deformation. The focus was the sand model, not the structural response of the test article. The sand material models utilized in the simulations were based on tests of sand specimens. Although the LS-DYNA models provided reasonable predictions for peak accelerations, they were not always able to track the response through the duration of the impact. Further improvements to the material model used for the sand were identified based on results from the sand specimen tests.
C1 [Vassilakos, Gregory J.] Analyt Mech Associates Inc, Hampton, VA 23666 USA.
[Vassilakos, Gregory J.; Hardy, Robin C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Vassilakos, GJ (reprint author), Analyt Mech Associates Inc, 21 Enterprise Pkwy,Ste 300, Hampton, VA 23666 USA.
EM gregory.j.vassilakos@nasa.gov; robin.c.hardy@nasa.gov
FU NASA Orion Program Office via the Landing and Descent Deceleration Earth
Recovery System (LADDERS); Structural Passive Landing Attenuation for
Survivability of Human Crew (SPLASH) projects
FX This paper describes work funded by the NASA Orion Program Office via
the Landing and Descent Deceleration Earth Recovery System (LADDERS) and
Structural Passive Landing Attenuation for Survivability of Human Crew
(SPLASH) projects.
NR 11
TC 1
Z9 1
U1 0
U2 6
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
EI 1943-5525
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD MAY 1
PY 2014
VL 27
IS 3
BP 442
EP 455
DI 10.1061/(ASCE)AS.1943-5525.0000365
PG 14
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA AE9RU
UT WOS:000334347400004
ER
PT J
AU Pereira, JM
Revilock, DM
Ruggeri, CR
Emmerling, WC
Altobelli, DJ
AF Pereira, J. Michael
Revilock, Duane M.
Ruggeri, Charles R.
Emmerling, William C.
Altobelli, Donald J.
TI Ballistic Impact Testing of Aluminum 2024 and Titanium 6Al-4V for
Material Model Development
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Material tests; Metals (materials); Material modeling; Impact tests
AB Ballistic impact testing was conducted on aluminum (Al) 2024 and titanium (Ti) 6Al-4Vanadium (V) sheet and plate samples of different thicknesses. The tests were conducted on flat panels with two different areal dimensions: 61x61 cm (24x24 in.) (large panel) and 38x38 cm (15x15 in.) (small panel), with projectile velocities between 150 and 300 m/s (500 and 1,000 ft/s). The smaller panels were impacted in a normal direction with cylindrical projectiles ranging in diameter from 1.27 cm to 1.91 cm (0.5 to 0.75 in.). The larger panels involved a more complex projectile, with some features representing those of real turbine engine fan blades, impacting the panel in an oblique orientation. For the large panels, data are reported on the impact velocity and whether the projectile penetrated the panel; for the small panels, data are reported on the residual velocities. For thick panels, friction between the projectile and the panel as the projectile translated through the panel appear to play a large role in penetration. Projectile hardness affects the penetration velocity. The data presented here provide a useful tool for developing and validating impact models.
C1 [Pereira, J. Michael; Revilock, Duane M.; Ruggeri, Charles R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Emmerling, William C.] Atlantic City Int Airport, Struct & Mat Sect ANG E231, Fed Aviat Adm William J Hughes Tech Ctr, Atlantic City, NJ 08405 USA.
[Altobelli, Donald J.] Atlantic City Int Airport, Fed Aviat Adm William J Hughes Tech Ctr, Atlantic City, NJ 08405 USA.
RP Pereira, JM (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM J.M.Pereira@nasa.gov; revilock@nasa.gov; charles.r.ruggeri@nasa.gov;
william.emmerling@faa.gov
NR 5
TC 1
Z9 1
U1 0
U2 2
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
EI 1943-5525
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD MAY 1
PY 2014
VL 27
IS 3
BP 456
EP 465
DI 10.1061/(ASCE)AS.1943-5525.0000356
PG 10
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA AE9RU
UT WOS:000334347400005
ER
PT J
AU Zhang, C
Binienda, WK
Kohlman, LW
AF Zhang, Chao
Binienda, Wieslaw K.
Kohlman, Lee W.
TI Analytical Model and Numerical Analysis of the Elastic Behavior of
Triaxial Braided Composites
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Finite-element analysis; Elastic behavior; Braided composite;
Undulation; Analytical model
ID WOVEN FABRIC COMPOSITES; TEXTILE COMPOSITES; STRENGTH; PREDICTION;
FAILURE
AB This paper is concerned with elastic behavior of a triaxial braided composite by using a three-dimensional analytical model and mesoscale finite-element (FE) analysis, in conjunction with experimental observations. The analytical method and FEM take into account the actual fabric structure by considering the fiber undulation and actual architecture parameters. A representative unit cell model of the triaxial braided architecture is first identified based on fiber volume ratio, specimen thickness, and microscopic image analysis. Detailed geometric parameters for axial and bias fiber bundles are obtained, which provide precise information to enable the development of analytical and FE models. A general three-dimensional analytical model based on realistic architecture is developed with consideration of axial and bias fiber undulation. A typical study on the effect of axial fiber undulation is presented through the analytical model and axial tensile test. The prediction of effective elastic constants of the composite are presented and are compared with the experimental data. Edge damage, which is identified through FE simulation and experiments, is found to occur periodically along the free edge and to result in reduced transverse properties. The edge effect on the elastic modulus is studied through FE simulation with various numbers of unit cells. The axial fiber undulation and edge effect explains the discrepancy between the analytical and computational predictions and the experimental results.
C1 [Zhang, Chao; Binienda, Wieslaw K.] Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
[Kohlman, Lee W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Zhang, C (reprint author), Univ Akron, Dept Civil Engn, Akron, OH 44325 USA.
EM cz14@zips.uakron.edu; wbinienda@uakron.edu; lee.w.kohlman@nasa.gov
RI Zhang, Chao/H-3397-2013
NR 36
TC 9
Z9 9
U1 4
U2 29
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
EI 1943-5525
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD MAY 1
PY 2014
VL 27
IS 3
BP 473
EP 483
DI 10.1061/(ASCE)AS.1943-5525.0000369
PG 11
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA AE9RU
UT WOS:000334347400007
ER
PT J
AU Wang, CX
Yang, P
Dessler, A
Baum, BA
Hu, YX
AF Wang, Chenxi
Yang, Ping
Dessler, Andrew
Baum, Bryan A.
Hu, Yongxiang
TI Estimation of the cirrus cloud scattering phase function from satellite
observations
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Thin cirrus clouds; Optical properties; Cloud phase function; Satellite
observations
ID TROPICAL THIN CIRRUS; ATMOSPHERIC INFRARED SOUNDER; LAND-SURFACE
TEMPERATURE; RADIATIVE-TRANSFER MODEL; OPTICAL-THICKNESS; MICROPHYSICAL
PROPERTIES; LIDAR MEASUREMENTS; WATER-VAPOR; ICE CLOUDS; PART II
AB Optical and microphysical properties for optically thin ice clouds are retrieved from one year of collocated Aqua/MODIS and CALIPSO/CALIOP measurements in 2008. The values of optical thickness tau and effective particle size D-eff are inferred from MODIS measurements at three infrared (IR) bands located at 8.5, 11, and 12 mu m in conjunction with collocated CALIOP cloud boundary altitudes and the MERRA atmospheric profile datasets. The values inferred from MODIS IR window measurements are insensitive to the pre-assumed particle and habit distributions. Based on near-IR measurements at 1.38 mu m and the IR-based tau, a new method is developed to infer the scattering phase functions over both ocean and land. A comparison between theoretically calculated phase functions and the retrieved counterparts demonstrates that roughened solid columns provide the best match for cirrus clouds over ocean, whereas droxtals may exist in optically thin cirrus clouds. The best-fitted phase functions are generated using appropriate habit mixtures to match the inferred phase functions. The phase function resulting from a mixture of 55% severely roughened solid columns, 35% severely roughened droxtals, and 10% smooth aggregates almost perfectly matches the mean phase function value retrieved over ocean. The asymmetry factor based on the oceanic best-fitted phase functions is 0.778 at a wavelength of 0.65 mu m. However, it is difficult to find an appropriate habit recipe to fit the inferred phase function over land. This may be caused by the relatively large uncertainties associated with tau retrievals over land. The retrieval of Deff shows that optically thin cirrus clouds consist of smaller ice particles in comparison with optically thicker ice clouds. The mean D-eff values of optically thin ice clouds over land and ocean are 41 mu m and 48 mu m, respectively. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Wang, Chenxi; Yang, Ping; Dessler, Andrew] 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.
[Hu, Yongxiang] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA USA.
RP Yang, P (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM pyang@tamu.edu
RI Baum, Bryan/B-7670-2011; Yang, Ping/B-4590-2011; Hu,
Yongxiang/K-4426-2012; Dessler, Andrew/G-8852-2012
OI Baum, Bryan/0000-0002-7193-2767; Dessler, Andrew/0000-0003-3939-4820
FU NASA grants [NNX10AM27G, NNX11AK37G, NNX11AF40G]; Texas A&M University
through the University of Wisconsin-Madison [301K630]
FX This study is supported by NASA grants NNX10AM27G, NNX11AK37G, and
NNX11AF40G (the associated subcontract to Texas A&M University through
the University of Wisconsin-Madison, 301K630). Bryan Baum and Ping Yang
thank Drs. Ramesh Kakar and Hal Maring for their encouragement and
support over the years.
NR 68
TC 6
Z9 6
U1 1
U2 14
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAY
PY 2014
VL 138
BP 36
EP 49
DI 10.1016/j.jqsrt.2014.02.001
PG 14
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AE6DR
UT WOS:000334081300003
ER
PT J
AU Nikitin, AV
Thomas, X
Regalia, L
Daumont, L
Rey, M
Tashkun, SA
Tyuterev, VG
Brown, LR
AF Nikitin, A. V.
Thomas, X.
Regalia, L.
Daumont, L.
Rey, M.
Tashkun, S. A.
Tyuterev, Vl. G.
Brown, L. R.
TI Measurements and modeling of long-path (CH4)-C-12 spectra in the
4800-5300 cm(-1) region
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Near infrared methane; Tetradecad; Long path FTIR; Transparency window;
Titan; Outer planets
ID M TRANSPARENCY WINDOW; HIGH-RESOLUTION SPECTROSCOPY; EMPIRICAL LINE
PARAMETERS; MIRS COMPUTER PACKAGE; MU-M; GLOBAL ANALYSIS; ROVIBRATIONAL
SPECTRA; INFRARED-SPECTROSCOPY; POLYATOMIC-MOLECULES; METHANE (CH4)-C-12
AB new study of (CH4)-C-12 line positions and intensities was performed for the lower portion of the Tetradecad region between 4800 and 5300 cm(-1) using long path (1603 m) spectra of normal sample CH4 at three pressures recorded with the Fourier transform spectrometer in Reims, France. Line positions and intensities were retrieved by least square curve-fitting procedures and analyzed using the effective Hamiltonian and the effective Dipole moment expressed in terms of irreducible tensor operators adapted to spherical top molecules. An existing spectrum of enriched (CH4)-C-13 was used to discern the isotopic lines. A new measured linelist produced positions and intensities for 5851 features (a factor of two more than prior work). Assignments were made for 46% of these; 2725 experimental line positions and 1764 selected line intensities were fitted with RMS standard deviations of 0.004 cm(-1) and 7.3%, respectively. The RMS of prior intensity fits of the lower Tetradecad was previously a factor of two worse. The sum of observed intensities between 4800 and 5300 cm(-1) fell within 5% of the predicted value from variational calculations. (c) 2014 Elsevier Ltd. All rights reserved.
C1 [Nikitin, A. V.; Tashkun, S. A.] SB RAS, VE Zuev Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634021, Russia.
[Thomas, X.; Regalia, L.; Daumont, L.; Rey, M.; Tyuterev, Vl. G.] Univ Reims, CNRS, UMR 7331, Grp Spectrometrie Mol & Atmospher, F-51687 Reims 2, France.
[Brown, L. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nikitin, A. V.] Tomsk State Univ, Tomsk 634050, Russia.
RP Nikitin, AV (reprint author), SB RAS, VE Zuev Inst Atmospher Opt, Lab Theoret Spect, 1 Acad Zuev Sq, Tomsk 634021, Russia.
EM avn@lts.iao.ru
RI Nikitin, Andrei/K-2624-2013; Tashkun, Sergey/E-8682-2014
OI Nikitin, Andrei/0000-0002-4280-4096;
FU Groupement de Recherche International SAMIA; CNRS (France); RFBR
(Russia); CAS (China); IDRIS\CINES computer centers of CNRS France;
computer center Reims-Champagne-Ardenne; PNP CNRS France
FX This work is part of the ANR project "CH4@Titan" (ref.:
BLAN08-2_321467). The support of the Groupement de Recherche
International SAMIA between CNRS (France), RFBR (Russia) and CAS (China)
is acknowledged. We acknowledge the support from IDRIS\CINES computer
centers of CNRS France and of the computer center
Reims-Champagne-Ardenne. The support of PNP CNRS France in frame of the
project "Study of isotopic methane bands in the 2 micron window for the
interpretation of space mission data" is acknowledged. A.N. thanks
computer centers of ICM@MG SB RAS (Novosibirsk) and SKIF Siberia
(Tomsk). Part of the research described in this paper was performed at
the Jet Propulsion Laboratory, California Institute of Technology, under
contracts with the National Aeronautics and Space Administration.
NR 58
TC 8
Z9 8
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD MAY
PY 2014
VL 138
BP 116
EP 123
DI 10.1016/j.jqsrt.2014.02.005
PG 8
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AE6DR
UT WOS:000334081300010
ER
PT J
AU Feldman, PD
Glenar, DA
Stubbs, TJ
Retherford, KD
Gladstone, GR
Miles, PF
Greathouse, TK
Kaufmann, DE
Parker, JW
Stern, SA
AF Feldman, Paul D.
Glenar, David A.
Stubbs, Timothy J.
Retherford, Kurt D.
Gladstone, G. Randall
Miles, Paul F.
Greathouse, Thomas K.
Kaufmann, David E.
Parker, Joel Wm.
Stern, S. Alan
TI Upper limits for a lunar dust exosphere from far-ultraviolet
spectroscopy by LRO/LAMP
SO ICARUS
LA English
DT Article
DE Moon; Atmospheres, evolution; Ultraviolet observations
ID ZODIACAL LIGHT; SCATTERING; MOON; LAMP
AB Since early 2012, the Lyman-Alpha Mapping Project (LAMP) far-ultraviolet spectrograph on the Lunar Reconnaissance Orbiter (LRO) spacecraft has carried out a series of limb observations from within lunar shadow to search for the presence of a high altitude dust exosphere via forward-scattering of sunlight from dust grains. Bright "horizon-glow" was observed from orbit during several Apollo missions and interpreted in terms of dust at altitudes of several km and higher. However, no confirmation of such an exosphere has been made since that time. This raises basic questions about the source(s) of excess brightness in the early measurements and also the conditions for producing observable dust concentrations at km altitudes and higher. Far-ultraviolet measurements between 170 and 190 nm, near the LAMP long wavelength cutoff, are especially sensitive to scattering by small (0.1-0.2 mu m radius) dust grains, since the scattering cross-section is near-maximum, and the solar flux is rising rapidly with wavelength. An additional advantage of ultraviolet measurements is the lack of interference by background zodiacal light which must be taken into account at longer wavelengths. As of July 2013, LAMP has completed several limb-observing sequences dedicated to the search for horizon glow, but no clear evidence of dust scattering has yet been obtained. Upper limits for vertical dust column abundance have been estimated at less than 10 grains cm(-2) (0.1 mu m grain radius), by comparing the measured noise-equivalent brightness with the results of Mie scattering simulations for the same observing geometries. These results indicate that Lunar Atmosphere Dust Environment Explorer (LADEE) UVS lunar dust observations will be considerably more challenging than planned. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Feldman, Paul D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Glenar, David A.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Stubbs, Timothy J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Retherford, Kurt D.; Gladstone, G. Randall; Miles, Paul F.; Greathouse, Thomas K.] SW Res Inst, San Antonio, TX 78228 USA.
[Kaufmann, David E.; Parker, Joel Wm.; Stern, S. Alan] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Glenar, David A.; Stubbs, Timothy J.] NASA, Ames Res Ctr, Lunar Sci Inst, Moffett Field, CA 94035 USA.
RP Feldman, PD (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
EM pdf@pha.jhu.edu
RI Stubbs, Timothy/I-5139-2013;
OI Stubbs, Timothy/0000-0002-5524-645X; Greathouse,
Thomas/0000-0001-6613-5731
FU NASA [NNG05EC87C]; Southwest Research Institute; NASA LASER Grant
[NNX09AO79G]; NASA Lunar Science Institute (NLSI/DREAM) [NNX09AG78A]
FX We thank the Lunar Reconnaissance Orbiter project team at NASA's Goddard
Space Flight Center for their continuous support. This work was
financially supported under contract NNG05EC87C from NASA to the
Southwest Research Institute. The work at Johns Hopkins University was
supported by a sub-contract from Southwest Research Institute. D. Glenar
and T. Stubbs were supported by NASA LASER Grant NNX09AO79G and by the
NASA Lunar Science Institute (NLSI/DREAM) under Grant NNX09AG78A.
NR 24
TC 13
Z9 13
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
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAY 1
PY 2014
VL 233
BP 106
EP 113
DI 10.1016/j.icarus.2014.01.039
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE1KX
UT WOS:000333729300010
ER
PT J
AU Cruikshank, DP
Ore, CMD
Clark, RN
Pendleton, YJ
AF Cruikshank, Dale P.
Ore, Cristina M. Dalle
Clark, Roger N.
Pendleton, Yvonne J.
TI Aromatic and aliphatic organic materials on Iapetus: Analysis of Cassini
VIMS data
SO ICARUS
LA English
DT Article
DE Iapetus; Organic chemistry; Satellites, composition; Saturn, satellites
ID DIFFUSE INTERSTELLAR-MEDIUM; INFRARED MAPPING SPECTROMETER; SATURNS MOON
PHOEBE; 3.4 MU-M; EMISSION FEATURES; IRREGULAR SATELLITES;
INTERPLANETARY DUST; SURFACE-COMPOSITION; HYDROCARBONS PAHS; ION
IRRADIATION
AB We present a quantitative analysis of the hydrocarbon and other organic molecular inventory as a component of the low-albedo material of Saturn's satellite Iapetus, based on a revision of the calibration of the Cassini VIMS instrument. Our study uses hyperspectral data from a mosaic of Iapetus' surface (Pinilla-Alonso, N., Roush, T.L., Marzo, G.A., Cruikshank, D.P., Dalle Ore, C.M. [2011]. Icarus 215, 75-82) constructed from VIMS data on a close fly-by of the satellite. We extracted 2235 individual spectra of the low-albedo regions, and with a clustering analysis tool (Dalle Ore, C.M., Cruikshank, D.P., Clark, R.N. 120121 Icarus 221, 735-743), separated them into two spectrally distinct groups, one concentrated on the leading hemisphere of Iapetus, and the other group on the trailing. This distribution is broadly consistent with that found from Cassini ISS data analyzed by Denk et al. (Denk, T. et al. [2010]. Science 327, 435-439). We modeled the average spectra of the two geographic regions using the materials and techniques described by Clark et al. (Clark, R.N., Cruikshank, D.P., Jaumann, R., Brown, R.H., Stephan, K, Dalle Ore, C.M., Livio, K.E., Pearson, N., Curchin, J.M., Hoefen, T.M., Buratti, B.J., Filacchione, G., Baines, ICH., Nicholson, P.D. [2012]. Icarus 218, 831-860), and after dividing the Iapetus spectrum by the model for each case, we extracted the resulting spectra in the interval 2.7-4.0 mu m for analysis of the organic molecular bands. The spectra reveal the C H stretching modes of aromatic hydrocarbons at similar to 3.28 mu m (similar to 3050 cm(-1)), plus four blended bands of aliphatic -CH2_- and -CH3 in the range similar to 3.36-3.52 mu m (similar to 2980-2840 cm(-1)). In these data, the aromatic band, probably indicating the presence of polycyclic aromatic hydrocarbons (PAR), is unusually strong in comparison to the aliphatic bands, as was found for Hyperion (Dalton, J.B., Cruikshank, D.P., Clark, R.N. [2012]. Icarus 220, 752-776; Dalle Ore, C.M., Cruikshank, D.P., Clark, R.N. [2012], op. cit.) and Phoebe (Dalle Ore, C.M., Cruikshank, D.P., Clark, R.N. [2012], op. cit.). Our Gaussian decomposition of the organic band region suggests the presence of molecular bands in addition to those noted above, specifically bands attributable to cycloalkanes, olefinic compounds, CH3OH, and N-substituted PAHs, as well as possible H-n-PAHs (PAHs with excess peripheral H atoms). In a minimalist interpretation of the Gaussian band fitting, we find the ratio of aromatic CH to aliphatic CH2 + CH3 functional groups for both the leading and trailing hemispheres of Iapetus is 10, with no clear difference between them. In the aliphatic component of the surface material, the ratio CH2/CH3 is 4.0 on the leading hemisphere and 3.0 on the trailing; both values are higher than those found in interstellar dust and other Solar System materials and the difference between the two hemispheres may be statistically significant. The superficial layer of low-albedo material on Iapetus originated in the interior of Phoebe and is being transported to and deposited on Iapetus (and Hyperion) in the current epoch via the Phoebe dust ring (Tosi, F., Turrini, D., Coradini, A., Filacchione, G., and the VIMS Team [2010]. Mon. Not. 1 Astron. Soc. 403, 1113-1130; Tamayo, D., Burns, J.A., Hamilton, D.P., Hedman, M.M. [2011]. Icarus 215, 260-278).
The PAHs on Iapetus exist in a H2O-rich environment, and consequently are subject to UV destruction by hydrogenation on short time-scales. The occurrence of this material is therefore consistent with the assertion that the deposition of the PAH-bearing dust is occurring at the present time. If the organic inventory we observe represents the interior composition of Phoebe, we may be sampling the original material from a region of the solar nebula beyond Neptune where Phoebe formed prior to its capture by Saturn (Johnson, T.V., Lunine, J.I. [2005]. Nature 435, 69-71). Published by Elsevier Inc.
C1 [Cruikshank, Dale P.; Ore, Cristina M. Dalle; Pendleton, Yvonne J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ore, Cristina M. Dalle] SETI Inst, Mountain View, CA 94043 USA.
[Clark, Roger N.] US Geol Survey, Denver, CO 80225 USA.
RP Cruikshank, DP (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM dale.p.cruikshank@nasa.gov
FU NASA Cassini project; VIMS team; Cassini Data Analysis program
FX We thank Drs. Hiroshi Imanaka, U. Allamandola, M.P. Bernstein, A.G.G.M.
Tielens, Diane H. Wooden, and especially S.A. Sandford for helpful
conversations as this work progressed. This work is supported in part by
the NASA Cassini project, the VIMS team, and Cassini Data Analysis
program (R. Clark and C.M. Dalle Ore, Principal Investigators).
NR 65
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U1 0
U2 15
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD MAY 1
PY 2014
VL 233
BP 306
EP 315
DI 10.1016/j.icarus.2014.02.011
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE1KX
UT WOS:000333729300026
ER
PT J
AU Reichle, RH
De Lannoy, GJM
Forman, BA
Draper, CS
Liu, Q
AF Reichle, Rolf H.
De Lannoy, Gabrielle J. M.
Forman, Barton A.
Draper, Clara S.
Liu, Qing
TI Connecting Satellite Observations with Water Cycle Variables Through
Land Data Assimilation: Examples Using the NASA GEOS-5 LDAS
SO SURVEYS IN GEOPHYSICS
LA English
DT Review
DE Land data assimilation; Land surface modeling; Satellite remote sensing;
Soil moisture; Snow; Terrestrial water storage; Ensemble Kalman filter
ID ENSEMBLE KALMAN FILTER; SURFACE DATA ASSIMILATION; CATCHMENT-BASED
APPROACH; 1997 FIELD EXPERIMENT; SOIL-MOISTURE; PASSIVE MICROWAVE; SNOW
DEPTH; MODEL; SYSTEM; EQUIVALENT
AB A land data assimilation system (LDAS) can merge satellite observations (or retrievals) of land surface hydrological conditions, including soil moisture, snow, and terrestrial water storage (TWS), into a numerical model of land surface processes. In theory, the output from such a system is superior to estimates based on the observations or the model alone, thereby enhancing our ability to understand, monitor, and predict key elements of the terrestrial water cycle. In practice, however, satellite observations do not correspond directly to the water cycle variables of interest. The present paper addresses various aspects of this seeming mismatch using examples drawn from recent research with the ensemble-based NASA GEOS-5 LDAS. These aspects include (1) the assimilation of coarse-scale observations into higher-resolution land surface models, (2) the partitioning of satellite observations (such as TWS retrievals) into their constituent water cycle components, (3) the forward modeling of microwave brightness temperatures over land for radiance-based soil moisture and snow assimilation, and (4) the selection of the most relevant types of observations for the analysis of a specific water cycle variable that is not observed (such as root zone soil moisture). The solution to these challenges involves the careful construction of an observation operator that maps from the land surface model variables of interest to the space of the assimilated observations.
C1 [Reichle, Rolf H.; De Lannoy, Gabrielle J. M.; Draper, Clara S.; Liu, Qing] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[De Lannoy, Gabrielle J. M.; Draper, Clara S.] Univ Space Res Assoc, Columbia, MD USA.
[Forman, Barton A.] Univ Maryland, Dept Civil & Environm Engn, College Pk, MD 20742 USA.
[Liu, Qing] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Reichle, RH (reprint author), NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Code 610-1,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM rolf.reichle@nasa.gov
RI Reichle, Rolf/E-1419-2012; Draper, Clara/P-6097-2016
OI Draper, Clara/0000-0002-8299-4939
FU NASA program on The Science of Terra and Aqua; NASA Soil Moisture Active
Passive mission; NASA Postdoctoral Program; NASA High-End Computing
program
FX The authors thank the organizers of the ISSI Workshop on "The Earth's
Hydrological Cycle" held February 6-10, 2012 and two anonymous reviewers
for their efforts. The research was supported by the NASA program on The
Science of Terra and Aqua, the NASA Soil Moisture Active Passive
mission, the NASA Postdoctoral Program, and the NASA High-End Computing
program.
NR 104
TC 19
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U1 3
U2 42
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-3298
EI 1573-0956
J9 SURV GEOPHYS
JI Surv. Geophys.
PD MAY
PY 2014
VL 35
IS 3
BP 577
EP 606
DI 10.1007/s10712-013-9220-8
PG 30
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AE1BN
UT WOS:000333700700006
ER
PT J
AU Lahoz, WA
De Lannoy, GJM
AF Lahoz, William A.
De Lannoy, Gabrielle J. M.
TI Closing the Gaps in Our Knowledge of the Hydrological Cycle over Land:
Conceptual Problems
SO SURVEYS IN GEOPHYSICS
LA English
DT Review
DE Hydrological cycle; Earth observation; Land surface models; Data
assimilation
ID SURFACE SOIL-MOISTURE; DATA ASSIMILATION SYSTEM; ENSEMBLE KALMAN FILTER;
VARIATIONAL DATA ASSIMILATION; NUMERICAL WEATHER-PREDICTION;
SNOW-COVERED AREA; MICROWAVE BRIGHTNESS TEMPERATURE; ERROR COVARIANCE
STATISTICS; ENVIRONMENT SIMULATOR JULES; INTEGRATED FORECAST SYSTEM
AB This paper reviews the conceptual problems limiting our current knowledge of the hydrological cycle over land. We start from the premise that to understand the hydrological cycle we need to make observations and develop dynamic models that encapsulate our understanding. Yet, neither the observations nor the models could give a complete picture of the hydrological cycle. Data assimilation combines observational and model information and adds value to both the model and the observations, yielding increasingly consistent and complete estimates of hydrological components. In this review paper we provide a historical perspective of conceptual problems and discuss state-of-the-art hydrological observing, modelling and data assimilation systems.
C1 [Lahoz, William A.] NILU, N-2027 Kjeller, Norway.
[Lahoz, William A.] Meteo France, CNRM GMGEC CARMA, F-31100 Toulouse, France.
[De Lannoy, Gabrielle J. M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Lahoz, WA (reprint author), NILU, Inst Veien 18,POB 100, N-2027 Kjeller, Norway.
EM wal@nilu.no; Gabrielle.Delannoy@nasa.gov
FU NILU internal project
FX This paper arose from the International Space Science Institute (ISSI)
workshop "The Earth's Hydrological Cycle", held at ISSI, Bern,
Switzerland, on 6-10 February 2012. A NILU internal project supported
WAL. Thanks to Alexandra Griesfeller for providing Fig. 2.
NR 292
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U1 4
U2 43
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-3298
EI 1573-0956
J9 SURV GEOPHYS
JI Surv. Geophys.
PD MAY
PY 2014
VL 35
IS 3
BP 623
EP 660
DI 10.1007/s10712-013-9221-7
PG 38
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AE1BN
UT WOS:000333700700008
ER
PT J
AU Foufoula-Georgiou, E
Ebtehaj, AM
Zhang, SQ
Hou, AY
AF Foufoula-Georgiou, E.
Ebtehaj, A. M.
Zhang, S. Q.
Hou, A. Y.
TI Downscaling Satellite Precipitation with Emphasis on Extremes: A
Variational l(1)-Norm Regularization in the Derivative Domain
SO SURVEYS IN GEOPHYSICS
LA English
DT Review
DE Sparsity; Inverse problems; l(1)-norm regularization; Non-smooth convex
optimization; Generalized Gaussian density; Extremes; Hurricanes
ID RESOLUTION TEMPORAL RAINFALL; MULTICOMPONENT DECOMPOSITION; ATOMIC
DECOMPOSITION; INVERSE PROBLEMS; BASIS PURSUIT; LARGE-SCALE; WAVELET;
SHRINKAGE; FIELDS; MODEL
AB The increasing availability of precipitation observations from space, e.g., from the Tropical Rainfall Measuring Mission (TRMM) and the forthcoming Global Precipitation Measuring (GPM) Mission, has fueled renewed interest in developing frameworks for downscaling and multi-sensor data fusion that can handle large data sets in computationally efficient ways while optimally reproducing desired properties of the underlying rainfall fields. Of special interest is the reproduction of extreme precipitation intensities and gradients, as these are directly relevant to hazard prediction. In this paper, we present a new formalism for downscaling satellite precipitation observations, which explicitly allows for the preservation of some key geometrical and statistical properties of spatial precipitation. These include sharp intensity gradients (due to high-intensity regions embedded within lower-intensity areas), coherent spatial structures (due to regions of slowly varying rainfall), and thicker-than-Gaussian tails of precipitation gradients and intensities. Specifically, we pose the downscaling problem as a discrete inverse problem and solve it via a regularized variational approach (variational downscaling) where the regularization term is selected to impose the desired smoothness in the solution while allowing for some steep gradients (called a""(1)-norm or total variation regularization). We demonstrate the duality between this geometrically inspired solution and its Bayesian statistical interpretation, which is equivalent to assuming a Laplace prior distribution for the precipitation intensities in the derivative (wavelet) space. When the observation operator is not known, we discuss the effect of its misspecification and explore a previously proposed dictionary-based sparse inverse downscaling methodology to indirectly learn the observation operator from a data base of coincidental high- and low-resolution observations. The proposed method and ideas are illustrated in case studies featuring the downscaling of a hurricane precipitation field.
C1 [Foufoula-Georgiou, E.] Univ Minnesota, Dept Civil Engn, St Anthony Falls Lab, Minneapolis, MN 55455 USA.
[Ebtehaj, A. M.] Univ Minnesota, Sch Math, Dept Civil Engn, St Anthony Falls Lab, Minneapolis, MN 55455 USA.
[Zhang, S. Q.; Hou, A. Y.] NASA, Goddard Space Flight Ctr, Greenbelt, MA USA.
RP Foufoula-Georgiou, E (reprint author), Univ Minnesota, Dept Civil Engn, St Anthony Falls Lab, Minneapolis, MN 55455 USA.
EM efi@umn.edu; ebteh001@umn.edu; sara.q.zhang@nasa.gov;
arthur.y.hou@nasa.gov
RI Measurement, Global/C-4698-2015
FU NASA-GPM award [NNX10AO12G]; NASA Earth and Space Science Fellowship
[NNX12AN45H]; Doctoral Dissertation Fellowship of the University of
Minnesota
FX This work has been mainly supported by a NASA-GPM award (NNX10AO12G), a
NASA Earth and Space Science Fellowship (NNX12AN45H), and a Doctoral
Dissertation Fellowship of the University of Minnesota to the second
author. The insightful comments of one anonymous referee are also
gratefully acknowledged.
NR 31
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Z9 5
U1 5
U2 22
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-3298
EI 1573-0956
J9 SURV GEOPHYS
JI Surv. Geophys.
PD MAY
PY 2014
VL 35
IS 3
BP 765
EP 783
DI 10.1007/s10712-013-9264-9
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AE1BN
UT WOS:000333700700013
ER
PT J
AU Bates, PD
Neal, JC
Alsdorf, D
Schumann, GJP
AF Bates, Paul D.
Neal, Jefferey C.
Alsdorf, Douglas
Schumann, Guy J-P
TI Observing Global Surface Water Flood Dynamics
SO SURVEYS IN GEOPHYSICS
LA English
DT Review
DE Floods; Surface water; Floodplains; Rivers; Wetlands; Remote sensing;
Surface water ocean topography (SWOT) mission
ID RADAR INTERFEROMETRY; SATELLITE RADAR; LEVEL CHANGES; DIGITAL
PHOTOGRAMMETRY; RIVER DISCHARGE; AMAZON RIVER; INUNDATION; ASSIMILATION;
ALTIMETRY; HYDROLOGY
AB Flood waves moving along river systems are both a key determinant of globally important biogeochemical and ecological processes and, at particular times and particular places, a major environmental hazard. In developed countries, sophisticated observing networks and ancillary data, such as channel bathymetry and floodplain terrain, exist with which to understand and model floods. However, at global scales, satellite data currently provide the only means of undertaking such studies. At present, there is no satellite mission dedicated to observing surface water dynamics and, therefore, surface water scientists make use of a range of sensors developed for other purposes that are distinctly sub-optimal for the task in hand. Nevertheless, by careful combination of the data available from topographic mapping, oceanographic, cryospheric and geodetic satellites, progress in understanding some of the world's major river, floodplain and wetland systems can be made. This paper reviews the surface water data sets available to hydrologists on a global scale and the recent progress made in the field. Further, the paper looks forward to the proposed NASA/CNES Surface Water Ocean Topography satellite mission that may for the first time provide an instrument that meets the needs of the hydrology community.
C1 [Bates, Paul D.; Neal, Jefferey C.] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
[Alsdorf, Douglas] Ohio State Univ, Sch Earth Sci, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
[Schumann, Guy J-P] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bates, PD (reprint author), Univ Bristol, Sch Geog Sci, Univ Rd, Bristol BS8 1SS, Avon, England.
EM paul.bates@bristol.ac.uk
RI Bates, Paul/C-8026-2012; Neal, Jeffrey/C-8723-2009; Schumann,
Guy/F-9760-2011
OI Bates, Paul/0000-0001-9192-9963; Neal, Jeffrey/0000-0001-5793-9594;
FU National Aeronautics and Space Administration
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.
NR 82
TC 15
Z9 15
U1 10
U2 55
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-3298
EI 1573-0956
J9 SURV GEOPHYS
JI Surv. Geophys.
PD MAY
PY 2014
VL 35
IS 3
BP 839
EP 852
DI 10.1007/s10712-013-9269-4
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AE1BN
UT WOS:000333700700016
ER
PT J
AU McGillivray, DA
Cravey, RL
Dudley, KL
Vedeler, E
Gupta, MC
AF McGillivray, Duncan A.
Cravey, Robin L.
Dudley, Kenneth L.
Vedeler, Erik
Gupta, Mool C.
TI POLARIZATION PROPERTIES OF A ONE DIMENSIONAL METAMATERIAL LENS
SO MICROWAVE AND OPTICAL TECHNOLOGY LETTERS
LA English
DT Article
DE metamaterials; split ring resonators; polarization; transmission;
sensors
ID NEGATIVE REFRACTION
AB The control of microwave (MW) radiation transmission through the polarization state of the incident beam is the basis for many applications in sensors and optics. Altering the polarization state of electromagnetic radiation by transmission through a metamaterial (MTM) lens could lead to novel devices and sensors. The polarization properties of 1D split ring resonator and rod type MTM structures were investigated and compared to a previously reported corresponding 2D MTM lens. Unlike the 2D lens, the 1D MTM did not contribute to a change in polarization state of transmitted MWs. The transmission response, however, was found to be determined by the coupling mechanisms between the MTMs constituent elements and orientation of the incident MW polarization. For the 1D lens, changing incident polarization from alignment parallel to the MTMs rod elements to alignment perpendicular to the rods, at resonance frequency, changes the effective index of refraction from net negative to positive. For a MTM structure, facing perpendicular to the incident radiation, the effective electromagnetic properties change from negative permittivity and positive permeability (for polarization parallel to the rod elements) to positive permittivity and negative permeability (for polarization perpendicular to the rod elements). (c) 2014 Wiley Periodicals, Inc. Microwave Opt Technol Lett 56:1218-1222, 2014
C1 [McGillivray, Duncan A.; Gupta, Mool C.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
[Cravey, Robin L.; Dudley, Kenneth L.; Vedeler, Erik] NASA, Langley Res Ctr, Electromagnet & Sensors Branch, Hampton, VA 23681 USA.
RP Gupta, MC (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
EM mgupta@virginia.edu
NR 16
TC 0
Z9 0
U1 2
U2 23
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0895-2477
EI 1098-2760
J9 MICROW OPT TECHN LET
JI Microw. Opt. Technol. Lett.
PD MAY
PY 2014
VL 56
IS 5
BP 1218
EP 1222
DI 10.1002/mop.28309
PG 5
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA AC4VP
UT WOS:000332519500049
ER
PT J
AU Ghisellini, G
Sbarrato, T
Tagliaferri, G
Foschini, L
Tavecchio, F
Ghirlanda, G
Braito, V
Gehrels, N
AF Ghisellini, G.
Sbarrato, T.
Tagliaferri, G.
Foschini, L.
Tavecchio, F.
Ghirlanda, G.
Braito, V.
Gehrels, N.
TI SDSS J114657.79+403708.6: the third most distant blazar at z=5.0
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; quasars: general; X-rays: general
ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; DATA RELEASE; BLACK-HOLES;
X-RAY; FERMI BLAZARS; LINE REGION; SWIFT; TELESCOPE; MISSION
AB The radio-loud quasar SDSS J114657.79+403708.6 at a redshift z = 5.0 is one of the most distant radio-loud objects. The IR-optical luminosity and spectrum suggest that its black hole has a very large mass: M = (5 +/- 1) x 10(9) M-circle dot. The radio-loudness (ratio of the radio to optical flux) of the source is large (around 100), suggesting that the source is viewed at small angles from the jet axis, and could be a blazar. The X-ray observations fully confirm this hypothesis, due to the high level and hardness of the flux. This makes SDSS J114657.79+403708.6 the third most distant blazar known, after Q0906+693 (z = 5.47) and B2 1023+25 (z = 5.3). Among those, SDSS J114657.79+403708.6 has the largest black holemass, setting interesting constraints on the mass function of heavy (>10(9)M(circle dot)) black holes at high redshifts.
C1 [Ghisellini, G.; Sbarrato, T.; Tagliaferri, G.; Foschini, L.; Tavecchio, F.; Ghirlanda, G.; Braito, V.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Sbarrato, T.] Univ Insubria, Dipartimento Fis & Matemat, I-22100 Como, Italy.
[Sbarrato, T.] ESO European Southern Observ, D-8578 Garching, Germany.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ghisellini, G (reprint author), INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy.
EM gabriele.ghisellini@brera.inaf.it
OI Braito, Valentina/0000-0002-2629-4989; Ghirlanda,
Giancarlo/0000-0001-5876-9259; Ghisellini, Gabriele/0000-0002-0037-1974;
Sbarrato, Tullia/0000-0002-3069-9399; Foschini,
Luigi/0000-0001-8678-0324; Tagliaferri, Gianpiero/0000-0003-0121-0723;
Tavecchio, Fabrizio/0000-0003-0256-0995
FU NASA
FX We thank the anonymous referee for useful comments. 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 NASA. Part of this work is based on archival data and online
service provided by the ASI Science Data Center (ASDC).
NR 38
TC 11
Z9 11
U1 0
U2 2
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 MAY 1
PY 2014
VL 440
IS 1
BP L111
EP L115
DI 10.1093/mnrasl/slu032
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CM8DM
UT WOS:000357927000023
ER
PT J
AU Ringerud, S
Kummerow, C
Peters-Lidard, C
Tian, YD
Harrison, K
AF Ringerud, Sarah
Kummerow, Christian
Peters-Lidard, Christa
Tian, Yudong
Harrison, Kenneth
TI A Comparison of Microwave Window Channel Retrieved and Forward-Modeled
Emissivities Over the US Southern Great Plains
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Emissivity; land surface; passive microwave remote sensing;
precipitation
ID LAND-SURFACE EMISSIVITIES; SOIL-MOISTURE; SATELLITE-OBSERVATIONS; DATA
ASSIMILATION; CLOUD DETECTION; UNITED-STATES; WATER-CONTENT; MODIS;
TEMPERATURE; RAINFALL
AB An accurate understanding of land surface emissivity in terms of associated surface properties is necessary for improved passive microwave remote sensing of the atmosphere, including water vapor, clouds, and precipitation, over land. In an effort to advance this understanding, emissivities are calculated for a 5 degrees latitude by 5 degrees longitude region in the U. S. Southern Great Plains using a combination of land surface model and physical emissivity model. Results are compared to retrieved values from the Advanced Microwave Scanning Radiometer-Earth Observing System passive microwave observations for cloud-free scenes over a six-year period. The resulting emissivities are compared in the context of surface properties including surface temperature, leaf area index (LAI), soil moisture, and precipitation. The comparison confirms that lower frequency channels respond most directly to the surface soil and its dielectric properties. Differences between retrieved and modeled emissivities are generally lower than 2%-3% and appear to be a function of soil moisture and LAI at frequencies less than 37 GHz. Agreement is better for the vertical polarization channels. At 89 GHz, a large difference is present between retrieved and modeled emissivities in both mean and magnitude of variability, particularly in the summer months. Problems are likely present at higher microwave frequencies in both the retrieved and modeled products, including the inability of the emissivity model to represent liquid water in the form of dew or precipitation interception on the vegetation canopy.
C1 [Ringerud, Sarah; Kummerow, Christian] Colorado State Univ, Ft Collins, CO 80523 USA.
[Peters-Lidard, Christa; Tian, Yudong; Harrison, Kenneth] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ringerud, S (reprint author), Colorado State Univ, Ft Collins, CO 80523 USA.
EM sarah@atmos.colostate.edu; kummerow@atmos.colostate.edu;
christa.d.peters-lidard@nasa.gov; yudong.tian-1@nasa.gov;
Kenneth.Harrison@nasa.gov
RI Peters-Lidard, Christa/E-1429-2012; Measurement, Global/C-4698-2015
OI Peters-Lidard, Christa/0000-0003-1255-2876;
FU Office of Science, Office of Biological and Environmental Research,
Climate and Environmental Sciences Division, U.S. Department of Energy
FX Data were obtained from the ARS Micronet program, operated and
maintained by the USDA Agricultural Research Service's Grazinglands
Research Laboratory, and from the Atmospheric Radiation Measurement
Program sponsored by the Office of Science, Office of Biological and
Environmental Research, Climate and Environmental Sciences Division,
U.S. Department of Energy.
NR 42
TC 10
Z9 10
U1 0
U2 11
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD MAY
PY 2014
VL 52
IS 5
BP 2395
EP 2412
DI 10.1109/TGRS.2013.2260759
PG 18
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA AC4IN
UT WOS:000332484700010
ER
PT J
AU Fore, AG
Yueh, SH
Tang, WQ
Hayashi, AK
Lagerloef, GSE
AF Fore, Alexander G.
Yueh, Simon H.
Tang, Wenqing
Hayashi, Akiko K.
Lagerloef, Gary S. E.
TI Aquarius Wind Speed Products: Algorithms and Validation
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aquarius; ocean winds; radar; remote sensing; scatterometery
ID BAND MICROWAVE OBSERVATIONS; SEA-SURFACE SALINITY; DIELECTRIC-CONSTANT;
TRIPLE COLLOCATION; SCATTEROMETER; SATELLITE; OCEAN; RETRIEVAL;
INSTRUMENT; STABILITY
AB This paper introduces and validates the Aquarius scatterometer-only wind speed algorithm and the combined active passive (CAP) wind speed products. The scatterometer-only algorithm uses the co-polarized radar cross-section to determine the ocean surface wind speed with a maximum-likelihood estimator approach while the CAP algorithm uses both the scatterometer and radiometer channels to achieve a simultaneous ocean vector wind and sea surface salinity retrieval. We discuss complications in the speed retrieval due to the shape of the scatterometer model function at L-band and develop mitigation strategies. We find the performance of the Aquarius scatterometer-only wind speed is better than 1.00 ms(-1), with best performance for low wind speeds and increasing noise levels as the wind speed increases. The CAP wind speed product is significantly better than the scatterometer-only due to the inclusion of passive measurements and achieves 0.70 ms(-1) root-mean-square error.
C1 [Fore, Alexander G.; Yueh, Simon H.; Tang, Wenqing; Hayashi, Akiko K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lagerloef, Gary S. E.] Earth & Space Res, Seattle, WA 98121 USA.
RP Fore, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Alexander.Fore@jpl.nasa.gov
FU National Aeronautics and Space Administration
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.
NR 26
TC 8
Z9 8
U1 0
U2 12
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 MAY
PY 2014
VL 52
IS 5
BP 2920
EP 2927
DI 10.1109/TGRS.2013.2267616
PG 8
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA AC4IN
UT WOS:000332484700052
ER
PT J
AU Wei, J
Savtchenko, A
Vollmer, B
Hearty, T
Albayrak, A
Crisp, D
Eldering, A
AF Wei, J.
Savtchenko, A.
Vollmer, B.
Hearty, T.
Albayrak, A.
Crisp, D.
Eldering, A.
TI Advances in CO2 Observations From AIRS and ACOS
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Carbon dioxide; infrared measurements; orbiting carbon observatory-2
(OCO-2); satellite application
ID ATMOSPHERIC CO2; RETRIEVAL ALGORITHM; SURFACE
AB NASA Goddard Earth Sciences Data and Information Services Center (GES DISC) archives and distributes pioneering collections of data on atmospheric greenhouse gases. In September of 2012, the Atmospheric Infrared Sounder (AIRS) marked a decade of tropospheric observations of carbon dioxide (CO2). Most recently, the Atmospheric CO2 Observations from Space (ACOS) project and GES DISC released CO2 retrievals derived from radiances observed by the Japanese Greenhouse gases Observing SATellite (GOSAT) satellite, launched in 2009. In this letter, we present the most recent estimates of decadal mid-tropospheric trends of CO2 from AIRS, as well as the most recent status of the total column-average distribution of CO2 from ACOS. We also demonstrate that significant discrepancies still exist in the global distribution of observed and modeled column amounts of CO2 using the CO2 retrievals from the ACOS project.
C1 [Wei, J.; Savtchenko, A.; Albayrak, A.] ADNET Syst Inc, Greenbelt, MD 20771 USA.
[Vollmer, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hearty, T.] Wyle Informat Syst, Greenbelt, MD 20771 USA.
[Crisp, D.; Eldering, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA.
RP Wei, J (reprint author), ADNET Syst Inc, Greenbelt, MD 20771 USA.
EM jennifer.c.wei@nasa.gov
FU NASA Earth Science Data and Information System (ESDIS) Project; National
Aeronautics and Space Administration
FX This work was supported by the NASA Earth Science Data and Information
System (ESDIS) Project. Part of the work described here was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
NR 21
TC 3
Z9 3
U1 2
U2 42
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 MAY
PY 2014
VL 11
IS 5
BP 891
EP 895
DI 10.1109/LGRS.2013.2281147
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 275WC
UT WOS:000328708000001
ER
PT J
AU Brunt, KM
Neumann, TA
Walsh, KM
Markus, T
AF Brunt, Kelly M.
Neumann, Thomas A.
Walsh, Kaitlin M.
Markus, Thorsten
TI Determination of Local Slope on the Greenland Ice Sheet Using a
Multibeam Photon-Counting Lidar in Preparation for the ICESat-2 Mission
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Airborne lidar; laser altimetry; photon counting
ID ELEVATION; ACCURACY
AB The greatest changes in elevation in Greenland and Antarctica are happening along the margins of the ice sheets where the surface frequently has significant slopes. For this reason, the upcoming Ice, Cloud, and land Elevation Satellite-2 (ICESat-2) mission utilizes pairs of laser altimeter beams that are perpendicular to the flight direction in order to extract slope information in addition to elevation. The Multiple Altimeter Beam Experimental Lidar (MABEL) is a high-altitude airborne laser altimeter designed as a simulator for ICESat-2. The MABEL design uses multiple beams at fixed angles and allows for local slope determination. Here, we present local slopes as determined by MABEL and compare them to those determined by the Airborne Topographic Mapper (ATM) over the same flight lines in Greenland. We make these comparisons with consideration for the planned ICESat-2 beam geometry. Results indicate that the mean slope residuals between MABEL and ATM remain small (< 0.05 degrees) through a wide range of localized slopes using ICESat-2 beam geometry. Furthermore, when MABEL data are subsampled by a factor of 4 to mimic the planned ICESat-2 transmit-energy configuration, the results are indistinguishable from the full-data-rate analysis. Results from MABEL suggest that ICESat-2 beam geometry and transmit-energy configuration are appropriate for the determination of slope on similar to 90-m spatial scales, a measurement that will be fundamental to deconvolving the effects of surface slope from the ice-sheet surface change derived from ICESat-2.
C1 [Brunt, Kelly M.] NASA, Goddard Space Flight Ctr, GESTAR, Greenbelt, MD 20771 USA.
[Neumann, Thomas A.; Markus, Thorsten] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Walsh, Kaitlin M.] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA.
RP Brunt, KM (reprint author), NASA, Goddard Space Flight Ctr, GESTAR, Greenbelt, MD 20771 USA.
EM kelly.m.brunt@nasa.gov
RI Neumann, Thomas/D-5264-2012
NR 18
TC 9
Z9 10
U1 4
U2 34
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 MAY
PY 2014
VL 11
IS 5
BP 935
EP 939
DI 10.1109/LGRS.2013.2282217
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 275WC
UT WOS:000328708000010
ER
PT J
AU Makishima, K
Enoto, T
Hiraga, JS
Nakano, T
Nakazawa, K
Sakurai, S
Sasano, M
Murakami, H
AF Makishima, K.
Enoto, T.
Hiraga, J. S.
Nakano, T.
Nakazawa, K.
Sakurai, S.
Sasano, M.
Murakami, H.
TI Possible Evidence for Free Precession of a Strongly Magnetized Neutron
Star in the Magnetar 4U 0142+61
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID X-RAY PULSARS; BOARD SUZAKU; FIELDS; SOFT; 4U-0142+61; EVOLUTION;
REPEATERS; RXTE
AB Magnetars are a special type of neutron stars, considered to have extreme dipole magnetic fields reaching similar to 10(11) T. The magnetar 4U 0142 + 61, one of the prototypes of this class, was studied in broadband x rays (0.5-70 keV) with the Suzaku observatory. In hard x rays (15-40 keV), its 8.69 sec pulsations suffered slow phase modulations by +/- 0.7 sec, with a period of similar to 15 h. When this effect is interpreted as free precession of the neutron star, the object is inferred to deviate from spherical symmetry by similar to 1.6 x 10(-4) in its moments of inertia. This deformation, when ascribed to magnetic pressure, suggests a strong toroidal magnetic field, similar to 10(12) T, residing inside the object. This provides one of the first observational approaches towards toroidal magnetic fields of magnetars.
C1 [Makishima, K.; Nakano, T.; Nakazawa, K.; Sakurai, S.; Sasano, M.; Murakami, H.] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Makishima, K.; Hiraga, J. S.] Univ Tokyo, Grad Sch Sci, Res Ctr Early Univ, Bunkyo Ku, Tokyo 1130033, Japan.
[Makishima, K.] RIKEN, MAXI Team, Wako, Saitama 3510198, Japan.
[Enoto, T.] RIKEN, Nishina Ctr, High Energy Astrophys Lab, Wako, Saitama 3510198, Japan.
[Enoto, T.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Makishima, K (reprint author), Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
RI XRAY, SUZAKU/A-1808-2009
FU MEXT [25105507]
FX This work was supported partially by the MEXT Grant-in-Aid for
Scientific Research on Innovative Areas, Area No. 2404, Grant No.
25105507.
NR 38
TC 22
Z9 22
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 30
PY 2014
VL 112
IS 17
AR 171102
DI 10.1103/PhysRevLett.112.171102
PG 5
WC Physics, Multidisciplinary
SC Physics
GA AH0NM
UT WOS:000335816700002
PM 24836230
ER
PT J
AU Brando, PM
Balch, JK
Nepstad, DC
Morton, DC
Putz, FE
Coe, MT
Silverio, D
Macedo, MN
Davidson, EA
Nobrega, CC
Alencar, A
Soares, BS
AF Brando, Paulo Monteiro
Balch, Jennifer K.
Nepstad, Daniel C.
Morton, Douglas C.
Putz, Francis E.
Coe, Michael T.
Silverio, Divino
Macedo, Marcia N.
Davidson, Eric A.
Nobrega, Caroline C.
Alencar, Ane
Soares-Filho, Britaldo S.
TI Abrupt increases in Amazonian tree mortality due to drought-fire
interactions
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE forest dieback; fireline intensity; stable states; MODIS; fire mapping
ID CLIMATE-CHANGE; RAIN-FORESTS; SAVANNA; SUSCEPTIBILITY; DEFORESTATION;
RESILIENCE; FEEDBACKS; BEHAVIOR; DIEBACK; TRAITS
AB Interactions between climate and land-use change may drive widespread degradation of Amazonian forests. High-intensity fires associated with extreme weather events could accelerate this degradation by abruptly increasing tree mortality, but this process remains poorly understood. Here we present, to our knowledge, the first field-based evidence of a tipping point in Amazon forests due to altered fire regimes. Based on results of a large-scale, longterm experiment with annual and triennial burn regimes (B1yr and B3yr, respectively) in the Amazon, we found abrupt increases in fire-induced tree mortality (226 and 462%) during a severe drought event, when fuel loads and air temperatures were substantially higher and relative humidity was lower than long-term averages. This threshold mortality response had a cascading effect, causing sharp declines in canopy cover (23 and 31%) and aboveground live biomass (12 and 30%) and favoring widespread invasion by flammable grasses across the forest edge area (80 and 63%), where fires were most intense (e. g., 220 and 820 kW.m(-1)). During the droughts of 2007 and 2010, regional forest fires burned 12 and 5% of southeastern Amazon forests, respectively, compared with < 1% in nondrought years. These results show that a few extreme drought events, coupled with forest fragmentation and anthropogenic ignition sources, are already causing widespread fire-induced tree mortality and forest degradation across southeastern Amazon forests. Future projections of vegetation responses to climate change across drier portions of the Amazon require more than simulation of global climate forcing alone and must also include interactions of extreme weather events, fire, and land-use change.
C1 [Brando, Paulo Monteiro; Silverio, Divino; Nobrega, Caroline C.; Alencar, Ane] Inst Pesquisa Ambiental Amazonia, BR-66035170 Belem, Para, Brazil.
[Brando, Paulo Monteiro; Coe, Michael T.; Macedo, Marcia N.; Davidson, Eric A.] Woods Hole Res Ctr, Falmouth, MA 02450 USA.
[Brando, Paulo Monteiro] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[Balch, Jennifer K.] Penn State Univ, Dept Geog, University Pk, PA 16802 USA.
[Nepstad, Daniel C.] Earth Innovat Inst, San Francisco, CA 94110 USA.
[Morton, Douglas C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Putz, Francis E.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA.
[Silverio, Divino] Univ Brasilia, Dept Ecol, BR-70910900 Brasilia, DF, Brazil.
[Nobrega, Caroline C.] Univ Fed Goias, Inst Ciencias Biol, BR-74001970 Goiania, Go, Brazil.
[Soares-Filho, Britaldo S.] Univ Fed Minas Gerais, Inst Geociencias, BR-6627 Belo Horizonte, MG, Brazil.
RP Brando, PM (reprint author), Inst Pesquisa Ambiental Amazonia, BR-66035170 Belem, Para, Brazil.
EM pmbrando@ipam.org.br
RI Morton, Douglas/D-5044-2012; Silverio, Divino Vicente/G-1154-2012;
Davidson, Eric/K-4984-2013; Brando, Paulo/C-4302-2012
OI Silverio, Divino Vicente/0000-0003-1642-9496; Davidson,
Eric/0000-0002-8525-8697; Brando, Paulo/0000-0001-8952-7025
FU Gordon and Betty Moore Foundation; National Science Foundation (Division
of Environmental Biology) [0410315, 0743703]; Packard Foundation;
National Aeronautics and Space Administration; Max Planck Institute for
Biogeochemistry
FX We thank S. Trumbore, Y. Malhi, C. A. Baldeck, and P. Cox for comments;
L. Curran and O. Carvalho for help with the experimental design; and
Instituto de Pesquisa Ambiental da Amazonia's field crew for taking
measurements. Grupo A. Maggi provided access to the field site and
logistical support. This study was supported by the Gordon and Betty
Moore Foundation, the National Science Foundation (Division of
Environmental Biology Grants 0410315 and 0743703), the Packard
Foundation, the National Aeronautics and Space Administration, and the
Max Planck Institute for Biogeochemistry.
NR 43
TC 98
Z9 99
U1 21
U2 137
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD APR 29
PY 2014
VL 111
IS 17
BP 6347
EP 6352
DI 10.1073/pnas.1305499111
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AG1TL
UT WOS:000335199000061
PM 24733937
ER
PT J
AU Gopalswamy, N
Akiyama, S
Yashiro, S
Xie, H
Makela, P
Michalek, G
AF Gopalswamy, Nat
Akiyama, Sachiko
Yashiro, Seiji
Xie, Hong
Maekelae, Pertti
Michalek, Grzegorz
TI Anomalous expansion of coronal mass ejections during solar cycle 24 and
its space weather implications
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE coronal mass ejections; anomalous expansion; geomagentic storms; solar
energetic particle events; space weather; solar cycle 24
ID ENERGETIC PARTICLE; INTENSITY; EVENTS
AB The familiar correlation between the speed and angular width of coronal mass ejections (CMEs) is also found in solar cycle 24, but the regression line has a larger slope: for a given CME speed, cycle 24 CMEs are significantly wider than those in cycle 23. The slope change indicates a significant change in the physical state of the heliosphere, due to the weak solar activity. The total pressure in the heliosphere (magnetic+plasma) is reduced by similar to 40%, which leads to the anomalous expansion of CMEs explaining the increased slope. The excess CME expansion contributes to the diminished effectiveness of CMEs in producing magnetic storms during cycle 24, both because the magnetic content of the CMEs is diluted and also because of the weaker ambient fields. The reduced magnetic field in the heliosphere may contribute to the lack of solar energetic particles accelerated to very high energies during this cycle.
C1 [Gopalswamy, Nat] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Akiyama, Sachiko; Yashiro, Seiji; Xie, Hong; Maekelae, Pertti] Catholic Univ Amer, Dept Phys, Washington, DE USA.
[Michalek, Grzegorz] Jagiellonian Univ, Astron Observ, Krakow, Poland.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM nat.gopalswamy@nasa.gov
OI Gopalswamy, Nat/0000-0001-5894-9954
FU NASA LWS TRT program
FX SOHO is a project of international cooperation between ESA and NASA.
This research was supported by NASA LWS TR&T program. We thank E.W.
Cliver and an anonymous referee for their constructive criticism, which
improved the presentation of the paper.
NR 24
TC 23
Z9 23
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 28
PY 2014
VL 41
IS 8
BP 2673
EP 2680
DI 10.1002/2014GL059858
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AH0KW
UT WOS:000335809800002
ER
PT J
AU Guan, B
Lee, T
Halkides, DJ
Waliser, DE
AF Guan, Bin
Lee, Tong
Halkides, Daria J.
Waliser, Duane E.
TI Aquarius surface salinity and the Madden-Julian Oscillation: The role of
salinity in surface layer density and potential energy
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Aquarius; salinity; MJO; satellite
ID MOIST THERMODYNAMIC STRUCTURE; INTRASEASONAL OSCILLATIONS; TROPICAL
CYCLONES; WESTERN PACIFIC; MJO; OCEAN; TEMPERATURE; CIRCULATION; MODEL;
VARIABILITY
AB Sea surface salinity (SSS) data from the Aquarius satellite are analyzed along with auxiliary data to investigate the SSS signature of the Madden-Julian Oscillation (MJO) in the equatorial Indian and Pacific Oceans, the effect of evaporation-minus-precipitation (E-P), the implication for the role of ocean dynamics, and the SSS influence on surface density and potential energy. MJO-related SSS changes are consistent with E-P forcing in the western Indian Ocean throughout the MJO cycle and in the central Indian Ocean during the wet phase of the MJO cycle. However, SSS changes cannot be explained by E-P in the central Indian Ocean during the dry phase and in the eastern Indian and western Pacific Oceans throughout the MJO cycle, implying the importance of ocean dynamics. SSS has an overall larger contribution to MJO-related surface density and potential energy anomalies than SST. It partially offsets the SST effect in the western-to-central Indian Ocean and reinforces the SST effect in the eastern Indian and western Pacific Oceans. Ocean modeling and assimilation need to properly account for salinity effects in order to correctly represent mixed layer variability associated with the MJO. Our results also clarify some discrepancy in previous studies about the E-P effect on MJO-related SSS variations.
Key Points
Clarifies role of E-P on MJO-related salinity and implication for ocean dynamics Corrects misinterpretation in a recent study about the role of E-P on salinity Reveals the important effects of salinity in surface layer density and energy
C1 [Guan, Bin; Halkides, Daria J.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Guan, Bin; Lee, Tong; Halkides, Daria J.; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Lee, T (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Tong.Lee@jpl.nasa.gov
RI Guan, Bin/F-6735-2010
FU National Aeronautics and Space Administration (NASA)
FX The research described in this paper was in part carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration (NASA).
NR 60
TC 8
Z9 8
U1 0
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 28
PY 2014
VL 41
IS 8
BP 2858
EP 2869
DI 10.1002/2014GL059704
PG 12
WC Geosciences, Multidisciplinary
SC Geology
GA AH0KW
UT WOS:000335809800026
ER
PT J
AU Ye, HC
Fetzer, EJ
Wong, S
Behrangi, A
Olsen, ET
Cohen, J
Lambrigtsen, BH
Chen, LK
AF Ye, Hengchun
Fetzer, Eric J.
Wong, Sun
Behrangi, Ali
Olsen, Edward T.
Cohen, Judah
Lambrigtsen, Bjorn H.
Chen, Luke
TI Impact of increased water vapor on precipitation efficiency over
northern Eurasia
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE atmospheric precipitable water; precipitation; relative humidity;
northern Eurasia; High latitudes; water vapor
ID HYDROLOGICAL CYCLE; TEMPERATURE; VARIABILITY; FREQUENCY; HUMIDITY;
TRENDS; MODEL; GCM
AB This study investigates the relationships among water vapor, precipitation efficiency, precipitation amount, and air temperature anomalies on monthly time scales over northern Eurasia for winter and summer 2003-2010. Daily precipitation and temperature records at 505 historical stations, and atmospheric total precipitable water vapor and relative humidity data from Atmospheric Infrared Sounders, are used for analysis. Results show that higher atmospheric precipitable water associated with warmer temperature directly contributes to winter precipitation amount but has little impact on winter precipitation efficiency. However, accelerated decreasing relative humidity associated with higher temperature is the primary factor in the reduction of precipitation efficiency and precipitation amount regardless of higher precipitable water in summer. This study suggests that there are evident seasonal differences in precipitation trend associated with air temperature changes over the study region. Air temperature modifies a key atmospheric water variable that directly controls precipitation for that particular season.
Key Points
Increasing water vapor directly contributes to winter precipitation Reduced summer precipitation is related to accelerated decreasing RH
C1 [Ye, Hengchun] Calif State Univ Los Angeles, Dept Geosci & Environm, Los Angeles, CA 90032 USA.
[Fetzer, Eric J.; Wong, Sun; Behrangi, Ali; Olsen, Edward T.; Lambrigtsen, Bjorn H.; Chen, Luke] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Cohen, Judah] Atmospher & Environm Res Inc, Lexington, MA USA.
RP Ye, HC (reprint author), Calif State Univ Los Angeles, Dept Geosci & Environm, Los Angeles, CA 90032 USA.
EM hye2@calstatela.edu
FU NSF [BCS-1060788]; JPL's Summer Faculty Fellow [BCS-1060323]
FX 5This research is supported by NSF grant BCS-1060788 and JPL's Summer
Faculty Fellow for HY; BCS-1060323 for JC. The authors wish to express
our gratitude toward the Carbon Dioxide Information Analysis Center for
providing the historical station precipitation data. We appreciate the
supportive comments and valuable suggestions from the three anonymous
reviewers that have improved the quality of this research.
NR 43
TC 7
Z9 8
U1 0
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 28
PY 2014
VL 41
IS 8
BP 2941
EP 2947
DI 10.1002/2014GL059830
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA AH0KW
UT WOS:000335809800037
ER
PT J
AU Zhao, YD
Chen, XM
Park, C
Fay, CC
Stupkiewicz, S
Ke, CH
AF Zhao, Yadong
Chen, Xiaoming
Park, Cheol
Fay, Catharine C.
Stupkiewicz, Stanislaw
Ke, Changhong
TI Mechanical deformations of boron nitride nanotubes in crossed junctions
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID INDIVIDUAL CARBON NANOTUBES; ELASTIC-MODULUS; WALLED CARBON; FORCE;
OXIDATION
AB We present a study of the mechanical deformations of boron nitride nanotubes (BNNTs) in crossed junctions. The structure and deformation of the crossed tubes in the junction are characterized by using atomic force microscopy. Our results show that the total tube heights are reduced by 20%-33% at the crossed junctions formed by double-walled BNNTs with outer diameters in the range of 2.21-4.67 nm. The measured tube height reduction is found to be in a nearly linear relationship with the summation of the outer diameters of the two tubes forming the junction. The contact force between the two tubes in the junction is estimated based on contact mechanics theories and found to be within the range of 4.2-7.6 nN. The Young's modulus of BNNTs and their binding strengths with the substrate are quantified, based on the deformation profile of the upper tube in the junction, and are found to be 1.07 +/- 0.11 TPa and 0.18-0.29 nJ/m, respectively. Finally, we perform finite element simulations on the mechanical deformations of the crossed BNNT junctions. The numerical simulation results are consistent with both the experimental measurements and the analytical analysis. The results reported in this paper contribute to a better understanding of the structural and mechanical properties of BNNTs and to the pursuit of their applications. (C) 2014 AIP Publishing LLC.
C1 [Zhao, Yadong; Chen, Xiaoming; Ke, Changhong] SUNY Binghamton, Dept Mech Engn, Binghamton, NY 13902 USA.
[Park, Cheol; Fay, Catharine C.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA.
[Stupkiewicz, Stanislaw] Inst Fundamental Technol Res, PL-00049 Warsaw, Poland.
RP Ke, CH (reprint author), SUNY Binghamton, Dept Mech Engn, Binghamton, NY 13902 USA.
EM cke@binghamton.edu
RI Ke, Changhong/C-4064-2008; Stupkiewicz, Stanislaw/J-8417-2012; CHEN,
XIAOMING/A-1377-2016
OI Stupkiewicz, Stanislaw/0000-0002-4592-3576;
FU U.S. Air Force Office of Scientific Research-Low Density Materials
program [FA9550-11-1-0042, FA9550-10-1-0451]; National Science Center
(NCN) in Poland [2011/01/B/ST8/07434]
FX This work was funded by U.S. Air Force Office of Scientific Research-Low
Density Materials program under Grant Nos. FA9550-11-1-0042 and
FA9550-10-1-0451. S.S. acknowledges the financial support of the
National Science Center (NCN) in Poland under Grant No.
2011/01/B/ST8/07434. The authors thank Dr. In-tae Bae for his assistance
with the TEM characterization. The TEM characterizations were performed
using the facilities in the Analytical and Diagnostics Laboratory at
Binghamton University's Small Scale Systems Integration and Packaging
Center (S3IP).
NR 46
TC 7
Z9 7
U1 2
U2 17
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
EI 1089-7550
J9 J APPL PHYS
JI J. Appl. Phys.
PD APR 28
PY 2014
VL 115
IS 16
AR 164305
DI 10.1063/1.4872238
PG 9
WC Physics, Applied
SC Physics
GA AG2EH
UT WOS:000335228400060
ER
PT J
AU Mocquet, A
Grasset, O
Sotin, C
AF Mocquet, A.
Grasset, O.
Sotin, C.
TI Very high-density planets: a possible remnant of gas giants
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
AND ENGINEERING SCIENCES
LA English
DT Article
DE exoplanets; internal structures; naked cores; gas giants; icy giants
ID MASS-RADIUS RELATIONSHIPS; SUPER-EARTHS; SOLID EXOPLANETS;
OCEAN-PLANETS; HIGH-PRESSURE; HOT JUPITERS; ATMOSPHERE; VISCOSITY
AB Data extracted from the Extrasolar Planets Encyclopaedia (see http://exoplanet.eu) show the existence of planets that are more massive than iron cores that would have the same size. After meticulous verification of the data, we conclude that the mass of the smallest of these planets is actually not known. However, the three largest planets, Kepler-52b, Kepler-52c and Kepler-57b, which are between 30 and 100 times the mass of the Earth, have indeed density larger than an iron planet of the same size. This observation triggers this study that investigates under which conditions these planets could represent the naked cores of gas giants that would have lost their atmospheres during their migration towards the star. This study shows that for moderate viscosity values (10(25) Pa s or lower), large values of escape rate and associated unloading stress rate during the atmospheric loss process lead to the explosion of extremely massive planets. However, for moderate escape rate, the bulk viscosity and finite-strain incompressibility of the cores of giant planets can be large enough to retain a very high density during geological time scales. This would make those a new kind of planet, which would help in understanding the interior structure of the gas giants. However, this new family of exoplanets adds some degeneracy for characterizing terrestrial exoplanets.
C1 [Mocquet, A.; Grasset, O.] Univ Nantes, CNRS, UMR 6112, LPG Nantes, F-44322 Nantes 03, France.
[Sotin, C.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Grasset, O (reprint author), Univ Nantes, CNRS, UMR 6112, LPG Nantes, 2 Rue Houssiniere, F-44322 Nantes 03, France.
EM olivier.grasset@univ-nantes.fr
NR 36
TC 2
Z9 2
U1 3
U2 11
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-503X
EI 1471-2962
J9 PHILOS T R SOC A
JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci.
PD APR 28
PY 2014
VL 372
IS 2014
AR 20130164
DI 10.1098/rsta.2013.0164
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AD6XM
UT WOS:000333404700016
PM 24664925
ER
PT J
AU Jin, ZH
Lukachin, C
Roberts, Y
Wielicki, B
Feldman, D
Collins, W
AF Jin, Zhonghai
Lukachin, Constantin
Roberts, Yolanda
Wielicki, Bruce
Feldman, Daniel
Collins, William
TI Interannual variability of the Earth's spectral solar reflectance from
measurements and simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE interannual variability; spectral solar reflectance; climate benchmark
ID MODELS; SYSTEM
AB The mean solar spectral reflectance averaged over large spatiotemporal scales is an important climate benchmark data product proposed for the Climate Absolute Radiance and Refractivity Observatory mission. The interannual variability of these reflectances over the ocean is examined through satellite-measured hyperspectral data and through satellite instrument emulation based on model simulation. Such large domain-averaged reflectances show small interannual variation, usually under few percent, depending on the latitude region and spatiotemporal scale used for averaging. Although the interannual variation is usually less than the absolute accuracy of model calculation, the model simulated interannual variations are consistent with the measurements because most of the modeling errors in the reflectance averaged in large climate domains are systematic and are canceled out in the interannual difference spectra. The interannual variability is also shown to decrease as the temporal and spatial scales increase. Both the observational data and the model simulations show that the natural variability in the annual mean reflectance is about 50% lower than that in the monthly mean over all spectra. The interannual variability determined from observations in large climate domains also compares favorably with that from the climate Observing System Simulation Experiment based on climate model simulations; both show a standard deviation of less than 1% of the mean reflectance across all spectra for global and annual average over the ocean.
Key Points Interannual variation of solar reflectance in large climate domains is small Simulated variation is consistent with hyperspectral satellite measurements Variance decreases as time/space scales increase, under 1% for global average
C1 [Jin, Zhonghai] Sci Syst & Applicat, Hampton, VA 23666 USA.
[Jin, Zhonghai; Lukachin, Constantin; Roberts, Yolanda; Wielicki, Bruce] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23665 USA.
[Feldman, Daniel; Collins, William] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Collins, William] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Climate Sci Dept, Berkeley, CA 94720 USA.
RP Jin, ZH (reprint author), Sci Syst & Applicat, Hampton, VA 23666 USA.
EM zhonghai.jin@nasa.gov
RI Collins, William/J-3147-2014; Richards, Amber/K-8203-2015; Feldman,
Daniel/N-8703-2013
OI Collins, William/0000-0002-4463-9848; Feldman,
Daniel/0000-0003-3365-5233
FU CLARREO project of NASA
FX We thank the SCIAMACHY team for the solar radiance data, the NASA CERES
group for the SSF data, and Sky Yang for the ozone data. The CERES SSF
data are available at the Atmospheric Science Data Center (ASDC) at NASA
Langley Research Center
(https://eosweb.larc.nasa.gov/project/ceres/ssf_table). The SCIAMACHY
data are provided through ESA by DLR
(http://atmos.caf.dlr.de/projects/scops/). The SMOBA ozone data are
provided by Sky Yang (Sk.Yang@noaa.gov) at NOAA. Amber Richards and
Rosemary Baize helped with the English editing. This research is
supported by the CLARREO project of NASA.
NR 19
TC 3
Z9 3
U1 1
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2014
VL 119
IS 8
BP 4458
EP 4470
DI 10.1002/2013JD021056
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AH0KP
UT WOS:000335809100002
ER
PT J
AU Yao, YJ
Liang, SL
Li, XL
Hong, Y
Fisher, JB
Zhang, NN
Chen, JQ
Cheng, J
Zhao, SH
Zhang, XT
Jiang, B
Sun, L
Jia, K
Wang, KC
Chen, Y
Mu, QZ
Feng, F
AF Yao, Yunjun
Liang, Shunlin
Li, Xianglan
Hong, Yang
Fisher, Joshua B.
Zhang, Nannan
Chen, Jiquan
Cheng, Jie
Zhao, Shaohua
Zhang, Xiaotong
Jiang, Bo
Sun, Liang
Jia, Kun
Wang, Kaicun
Chen, Yang
Mu, Qiaozhen
Feng, Fei
TI Bayesian multimodel estimation of global terrestrial latent heat flux
from eddy covariance, meteorological, and satellite observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Review
DE latent heat flux; evapotranspiration; Bayesian model averaging method;
simple model averaging method
ID REFLECTANCE DISTRIBUTION FUNCTION; LAND-SURFACE EVAPORATION;
ENERGY-BALANCE CLOSURE; NET PRIMARY PRODUCTION; SOUTHERN GREAT-PLAINS;
REMOTELY-SENSED DATA; CARBON-DIOXIDE; EVAPOTRANSPIRATION ALGORITHM;
ALBEDO RETRIEVALS; BOREAL FOREST
AB Accurate estimation of the satellite-based global terrestrial latent heat flux (LE) at high spatial and temporal scales remains a major challenge. In this study, we introduce a Bayesian model averaging (BMA) method to improve satellite-based global terrestrial LE estimation by merging five process-based algorithms. These are the Moderate Resolution Imaging Spectroradiometer (MODIS) LE product algorithm, the revised remote-sensing-based Penman-Monteith LE algorithm, the Priestley-Taylor-based LE algorithm, the modified satellite-based Priestley-Taylor LE algorithm, and the semi-empirical Penman LE algorithm. We validated the BMA method using data for 2000-2009 and by comparison with a simple model averaging (SA) method and five process-based algorithms. Validation data were collected for 240 globally distributed eddy covariance tower sites provided by FLUXNET projects. The validation results demonstrate that the five process-based algorithms used have variable uncertainty and the BMA method enhances the daily LE estimates, with smaller root mean square errors (RMSEs) than the SA method and the individual algorithms driven by tower-specific meteorology and Modern Era Retrospective Analysis for Research and Applications (MERRA) meteorological data provided by the NASA Global Modeling and Assimilation Office (GMAO), respectively. The average RMSE for the BMA method driven by daily tower-specific meteorology decreased by more than 5 W/m(2) for crop and grass sites, and by more than 6 W/m(2) for forest, shrub, and savanna sites. The average coefficients of determination (R-2) increased by approximately 0.05 for most sites. To test the BMA method for regional mapping, we applied it for MODIS data and GMAO-MERRA meteorology to map annual global terrestrial LE averaged over 2001-2004 for spatial resolution of 0.05 degrees. The BMA method provides a basis for generating a long-term global terrestrial LE product for characterizing global energy, hydrological, and carbon cycles.
Key Points BMA-based latent heat flux estimation Global terrestrial LE estimation Integrating five process-based algorithms
C1 [Yao, Yunjun; Liang, Shunlin; Li, Xianglan; Cheng, Jie; Zhang, Xiaotong; Jiang, Bo; Jia, Kun; Feng, Fei] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China.
[Liang, Shunlin] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Hong, Yang] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA.
[Hong, Yang] Tsinghua Univ, Dept Hydraul Engn, Beijing 100084, Peoples R China.
[Hong, Yang] Tsinghua Univ, State Key Lab Hydrosci & Engn, Beijing 100084, Peoples R China.
[Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Zhang, Nannan] Hohai Univ, Sch Earth Sci & Engn, Nanjing, Jiangsu, Peoples R China.
[Chen, Jiquan] Univ Toledo, Dept Environm Sci, Toledo, OH 43606 USA.
[Zhao, Shaohua] Minist Environm Protect, Environm Satellite Ctr, Beijing, Peoples R China.
[Sun, Liang] Chinese Acad Agr Sci, Inst Agr Resources & Reg Planning, Beijing 100193, Peoples R China.
[Wang, Kaicun; Chen, Yang] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, State Key Lab Earth Surface Proc & Resource Ecol, Beijing 100875, Peoples R China.
[Mu, Qiaozhen] Univ Montana, Dept Ecosyst & Conservat Sci, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA.
RP Yao, YJ (reprint author), Beijing Normal Univ, Coll Global Change & Earth Syst Sci, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China.
EM boyyunjun@163.com; xlli@bnu.edu.cn
RI rslab, water/O-7043-2015; Wang, Kaicun/F-7813-2012; Cheng,
Jie/G-2039-2011; Chen, Jiquan/D-1955-2009; Hong, Yang/D-5132-2009; Mu,
Qiaozhen/G-5695-2010; liang, shunlin/C-2809-2015; rslab,
hiwater/O-7037-2015
OI Wang, Kaicun/0000-0002-7414-5400; Fisher, Joshua/0000-0003-4734-9085;
Hong, Yang/0000-0001-8720-242X;
FU U.S. Department of Energy, Biological and Environmental Research,
Terrestrial Carbon Program [DE-FG02-04ER63917, DE-FG02-04ER63911];
CFCAS; NSERC; BIOCAP; Environment Canada; NRCan; CarboEuropeIP;
FAO-GTOS-TCO; iLEAPS; Max Planck Institute for Biogeochemistry; National
Science Foundation; University of Tuscia; Universite Laval; U.S.
Department of Energy; High-Tech Research and Development Program of
China [2013AA122801]; Natural Science Fund of China [41201331, 41101310,
41101313, 41301353, 41205104]; National Basic Research Program of China
[2012CB955302]; Fundamental Research Funds for the Central Universities
[2013YB34]; High Resolution Earth Observation Systems of National
Science and Technology Major Projects [05-Y30B02-9001-13/15-9]; National
Aeronautics and Space Administration
FX Authors thank the three anonymous reviewers for their critical and
helpful comments and suggestions. Authors also thank Shaomin Liu,
Wenping Yuan, and Ziwei Xu from Beijing Normal University, China;
Guangsheng Zhou from the Institute of Botany, CAS; Yan Li and Ran Liu
from Xinjiang Institute of Ecology and Geography, CAS; Guoyi Zhou and
Yuelin Li from South China Botanic Garden, CAS; and Bin Zhao from Fudan
University, China, for providing ground-measured data. This work used
eddy covariance data acquired by the FLUXNET community and, in
particular, by the following networks: AmeriFlux (U.S. Department of
Energy, Biological and Environmental Research, Terrestrial Carbon
Program (DE-FG02-04ER63917 and DE-FG02-04ER63911)), AfriFlux, AsiaFlux,
CarboAfrica, CarboEuropeIP, CarboItaly, CarboMont, ChinaFlux,
Fluxnet-Canada (supported by CFCAS, NSERC, BIOCAP, Environment Canada,
and NRCan), GreenGrass, KoFlux, LBA, NECC, OzFlux, TCOS-Siberia, and
USCCC. We acknowledge the financial support to the eddy covariance data
harmonization provided by CarboEuropeIP, FAO-GTOS-TCO, iLEAPS, Max
Planck Institute for Biogeochemistry, National Science Foundation,
University of Tuscia, Universite Laval, Environment Canada, and U.S.
Department of Energy, and the database development and technical support
from Berkeley Water Center, Lawrence Berkeley National Laboratory,
Microsoft Research eScience, Oak Ridge National Laboratory, University
of California-Berkeley, and the University of Virginia. Other
ground-measured data were obtained from the GAME ANN
(http://aan.suiri.tsukuba.ac.jp/), the Coordinated Enhanced Observation
Project (CEOP) in arid and semiarid regions of northern China
(http://observation.tea.ac.cn/), and the water experiments of
Environmental and Ecological Science Data Center for West China
(http://westdc.westgis.ac.cn/water). MODIS LAI/FPAR, NDVI, albedo, and
land cover satellite products were obtained online
(http://reverb.echo.nasa.gov/reverb). This work was partially supported
by the High-Tech Research and Development Program of China
(2013AA122801), the Natural Science Fund of China (41201331, 41101310,
41101313, 41301353, and 41205104), the National Basic Research Program
of China (2012CB955302), the Fundamental Research Funds for the Central
Universities (2013YB34), the High Resolution Earth Observation Systems
of National Science and Technology Major Projects
(05-Y30B02-9001-13/15-9). J.B.F. contributed to this paper from the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 105
TC 17
Z9 18
U1 5
U2 67
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2014
VL 119
IS 8
BP 4521
EP 4545
DI 10.1002/2013JD020864
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AH0KP
UT WOS:000335809100007
ER
PT J
AU Tang, L
Tian, YD
Lin, X
AF Tang, Ling
Tian, Yudong
Lin, Xin
TI Validation of precipitation retrievals over land from satellite- based
passive microwave sensors
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE satellite precipitation; error; passive microwave
ID LATENT HEATING DISTRIBUTIONS; CONTINENTAL UNITED-STATES; OCEAN RAIN
RATE; PHYSICAL RETRIEVALS; SOUNDING UNIT; ALGORITHMS; RESOLUTION;
PRODUCTS; CLOUD; IMAGER/SOUNDER
AB Precipitation retrievals from spaceborne passive microwave (PMW) radiometers are the backbone of modern satellite-based global precipitation data sets. The error characteristics in these individual retrievals directly affect the merged end products and applications but have not been systematically studied. This paper focuses on extensive and systematic validation of PMW precipitation retrievals and quantification of their error characteristics. Retrievals from 12 PMW radiometers were evaluated and intercompared at instantaneous scale (5min) over continental United States. These precipitation-sensing radiometers include both imagers (Tropical Rainfall Measuring Mission Microwave Imager, Advanced Microwave Scanning Radiometer for the Earth Observing System, Special Sensor Microwave Imager, and Special Sensor Microwave Imager/Sounder) and sounders (advanced microwave sounding unit-B and Microwave Humidity Sounders). A high-resolution ground radar-based data set over the continental United States was used as the ground reference data. The high spatial and temporal resolution of the reference data allows collocation within 5min and relatively more precise comparison with the satellite overpasses. Our results show that PMW sensor retrievals exhibit fairly systematic biases depending on season and precipitation intensity, with overestimates in summer at moderate to high precipitation rates and underestimates in winter at low and moderate precipitation rates. Retrievals from the microwave imagers have notably better performance than those from the sounders. The latter tend to have a narrower dynamic range, higher biases, and random errors.
Key Points Extensive and systematic validation for L2 precipitation retrievals from PMWs Fairly systematic biases Imagers have notably better performance than the sounders
C1 [Tang, Ling; Tian, Yudong; Lin, Xin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Tang, Ling; Tian, Yudong; Lin, Xin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Tang, L (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM ltang21@umd.edu
RI Measurement, Global/C-4698-2015
FU NASA Earth System Data Records Uncertainty Analysis Program
[NNH10ZDA001N-ESDRERR]
FX This research was supported by the NASA Earth System Data Records
Uncertainty Analysis Program (Martha E. Maiden) under solicitation
NNH10ZDA001N-ESDRERR. Computing resources were provided by the NASA
Center for Climate Simulation. We appreciate the assistance and advice
from Bob Adler, Bob Joyce, Eric Nelkin, Daniel Vila, Huan Meng, Nai-Yu
Wang, and Jun Dong. Helpful comments and suggestions from three
anonymous reviewers are gratefully acknowledged.
NR 51
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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 APR 27
PY 2014
VL 119
IS 8
BP 4546
EP 4567
DI 10.1002/2013JD020933
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AH0KP
UT WOS:000335809100008
ER
PT J
AU Dumka, UC
Tripathi, SN
Misra, A
Giles, DM
Eck, TF
Sagar, R
Holben, BN
AF Dumka, U. C.
Tripathi, S. N.
Misra, Amit
Giles, D. M.
Eck, T. F.
Sagar, Ram
Holben, B. N.
TI Latitudinal variation of aerosol properties from IndoGangetic Plain to
central Himalayan foothills during TIGERZ campaign
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Central Himalayas; heating rate; aerosol radiative forcing; aerosol
optical properites; TIGERZ
ID INDO-GANGETIC BASIN; SKY RADIANCE MEASUREMENTS; TROPICAL INDIAN-OCEAN;
OPTICAL-PROPERTIES; NORTHERN INDIA; ORGANIC-CARBON; DUST STORMS;
AERONET; DEPTH; ABSORPTION
AB As part of TIGERZ campaign, latitudinal variation of aerosol optical properties was analyzed over Indo-Gangetic Plains (IGP) to central Himalayas during premonsoon of 2008 and 2009. Measurements of aerosol optical depth (AOD) were performed using Aerosol Robotic Network Sun photometer at four sites with different aerosol environments. The AOD increases from Nainital located in central Himalayas to Kanpur located in IGP region. Further, aerosol size varies spatially with dominance of coarse-mode aerosols at Kanpur compared to fine-mode aerosols dominated at Nainital. Spectral variation of single-scattering albedo suggests that during premonsoon, dust is the dominant species in the IGP with exception of Pantnagar, where absorbing aerosols are dominant. The optical properties of aerosols are calculated, and shortwave clear-sky aerosol radiative forcing (ARF) is estimated. An insignificant difference is found in columnar ARF and columnar heating rate (HR) when vertical profiles of aerosols are included in radiative transfer models. Over Nainital, average ARF is estimated to be -7.61, -45.75, and 38.14Wm(-2) at top of atmosphere (TOA), surface (SUR), and in the atmosphere (ATM), respectively. Average ARF is less negative at Kanpur compared to Pantnagar and Bareilly with values -17.63, -73.06, and 55.43Wm(-2) at TOA, SUR, and ATM, respectively. ARF shows positive gradient from the highlands to the IGP sites; larger TOA and SUR cooling were observed at the three sites compared to the highland site. This translates into large columnar HR with estimated average values as 1.07, 1.41, 1.58, and 1.56 Kd(-1) for Nainital, Pantnagar, Bareilly, and Kanpur, respectively.
C1 [Dumka, U. C.; Sagar, Ram] Aryabhatta Res Inst Observat Sci, Naini Tal, India.
[Tripathi, S. N.; Misra, Amit] Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India.
[Giles, D. M.] Sigma Space Corp, Lanham, MD USA.
[Giles, D. M.; Eck, T. F.; Holben, B. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Eck, T. F.] Univ Space Res Assoc, Columbia, MD USA.
RP Dumka, UC (reprint author), Aryabhatta Res Inst Observat Sci, Naini Tal, India.
EM dumka@aries.res.in; snt@iitk.ac.in
RI Dumka, Umesh /D-3520-2015; Tripathi, Sachchida/J-4840-2016
OI Dumka, Umesh /0000-0001-9448-1543;
FU National Academy of Science; U.S. Agency for International Development
FX The authors thank the editor and anonymous reviewers for their valuable
comments and suggestions which significantly improved the paper. A part
of this work was supported by National Academy of Science and U.S.
Agency for International Development. The authors would like to
acknowledge Harish Vishwakarma at IIT-Kanpur for field support during
TIGERZ. The authors thank the AERONET team for calibrating and
maintaining the instrument and processing the data. The NCEP reanalysis
data are obtained from http://www.cdc.noaa.gov, and CALIPSO extinction
coefficients are obtained from
http://www-calipso.larc.nasa.gov/tools/data_avail/.
NR 66
TC 15
Z9 15
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2014
VL 119
IS 8
BP 4750
EP 4769
DI 10.1002/2013JD021040
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AH0KP
UT WOS:000335809100020
ER
PT J
AU Douglass, AR
Strahan, SE
Oman, LD
Stolarski, RS
AF Douglass, A. R.
Strahan, S. E.
Oman, L. D.
Stolarski, R. S.
TI Understanding differences in chemistry climate model projections of
stratospheric ozone
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE stratospheric ozone; chemistry climate models
ID MIDDLE ATMOSPHERE; CHLORINE PERTURBATIONS; INORGANIC CHLORINE; TRANSPORT
MODEL; TECHNICAL NOTE; TRENDS; CLONO2; SENSITIVITY; HCL; PHOTOCHEMISTRY
AB Chemistry climate models (CCMs) are used to project future evolution of stratospheric ozone as concentrations of ozone-depleting substances (ODSs) decrease and greenhouse gases increase, cooling the stratosphere. CCM projections exhibit not only many common features but also a broad range of values for quantities such as year of ozone return to 1980 and global ozone level at the end of the 21st century. Multiple linear regression is applied to each of 14 CCMs to separate ozone response to ODS concentration change from that due to climate change. We show that the sensitivity of lower stratospheric ozone to chlorine change O-3/Cl-y is a near-linear function of partitioning of total inorganic chlorine (Cl-y) into its reservoirs; both Cl-y and its partitioning are largely controlled by lower stratospheric transport. CCMs with best performance on transport diagnostics agree with observations for chlorine reservoirs and produce similar ozone responses to chlorine change. After 2035, differences in O-3/Cl-y contribute little to the spread in CCM projections as the anthropogenic contribution to Cl-y becomes unimportant. Differences among upper stratospheric ozone increases due to temperature decreases are explained by differences in ozone sensitivity to temperature change O-3/T due to different contributions from various ozone loss processes, each with its own temperature dependence. Ozone decrease in the tropical lower stratosphere caused by a projected speedup in the Brewer-Dobson circulation may or may not be balanced by ozone increases in the middle- and high-latitude lower stratosphere and upper troposphere. This balance, or lack thereof, contributes most to the spread in late 21st century projections.
C1 [Douglass, A. R.; Oman, L. D.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Strahan, S. E.] Univ Space Res Assoc, Columbia, MD USA.
[Stolarski, R. S.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
RP Douglass, AR (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Anne.R.Douglass@nasa.gov
RI Douglass, Anne/D-4655-2012; Stolarski, Richard/B-8499-2013; Oman,
Luke/C-2778-2009
OI Stolarski, Richard/0000-0001-8722-4012; Oman, Luke/0000-0002-5487-2598
FU NASA's Atmospheric Chemistry Modeling and Analysis Program (ACMAP);
Modeling and Analysis Program (MAP)
FX We acknowledge the modeling groups for making their simulations
available for this analysis. The Chemistry-Climate Model Validation
Activity (CCMVal) for WCRP's (World Climate Research Programme) SPARC
(Stratosphere-troposphere Processes and their Role in Climate) project
for organizing and coordinating the model data analysis activity and the
British Atmospheric Data Center (BADC) for collecting and archiving the
CCMVal model output. The data used in this publication were obtained as
part of the Network for the Detection of Atmospheric Composition Change
(NDACC) and are publicly available (see http://www.ndacc.org). We
appreciate helpful comments from three anonymous reviewers. This work is
supported by NASA's Atmospheric Chemistry Modeling and Analysis Program
(ACMAP) and Modeling and Analysis Program (MAP).
NR 58
TC 3
Z9 3
U1 1
U2 19
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2014
VL 119
IS 8
BP 4922
EP 4939
DI 10.1002/2013JD021159
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AH0KP
UT WOS:000335809100030
ER
PT J
AU Divakarla, M
Barnet, C
Liu, X
Gu, DG
Wilson, M
Kizer, S
Xiong, XZ
Maddy, E
Ferraro, R
Knuteson, R
Hagan, D
Ma, XL
Tan, CY
Nalli, N
Reale, A
Mollner, AK
Yang, WZ
Gambacorta, A
Feltz, M
Iturbide-Sanchez, F
Sun, BM
Goldberg, M
AF Divakarla, Murty
Barnet, Christopher
Liu, Xu
Gu, Degui
Wilson, Michael
Kizer, Susan
Xiong, Xiaozhen
Maddy, Eric
Ferraro, Ralph
Knuteson, Robert
Hagan, Denise
Ma, Xia-lin
Tan, Changyi
Nalli, Nicholas
Reale, Anthony
Mollner, Andrew K.
Yang, Wenze
Gambacorta, Antonia
Feltz, Michelle
Iturbide-Sanchez, Flavio
Sun, Bomin
Goldberg, Mitch
TI The CrIMSS EDR Algorithm: Characterization, Optimization, and Validation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE CrIMSS; CrIS; ATMS; EDR
ID INFRARED SOUNDER TEMPERATURE; TERRESTRIAL MATERIALS; ATMOSPHERIC WINDOW;
RADIO OCCULTATION; PRODUCTS; WEATHER; AIRS/AMSU/HSB; RETRIEVALS;
EMISSIVITY; CLIMATE
AB The Cross-track Infrared Sounder (CrIS) and the Advanced Technology Microwave Sounder (ATMS) instruments aboard the Suomi National Polar-orbiting Partnership satellite provide high-quality hyperspectral infrared and microwave observations to retrieve atmospheric vertical temperature and moisture profiles (AVTP and AVMP) and many other environmental data records (EDRs). The official CrIS and ATMS EDR algorithm, together called the Cross-track Infrared and Microwave Sounding Suite (CrIMSS), produces EDR products on an operational basis through the interface data processing segment. The CrIMSS algorithm group is to assess and ensure that operational EDRs meet beta and provisional maturity requirements and are ready for stages 1-3 validations. This paper presents a summary of algorithm optimization efforts, as well as characterization and validation of the AVTP and AVMP products using the European Centre for Medium-Range Weather Forecasts (ECMWF) analysis, the Atmospheric Infrared Sounder (AIRS) retrievals, and conventional and dedicated radiosonde observations. The global root-mean-square (RMS) differences between the CrIMSS products and the ECMWF show that the AVTP is meeting the requirements for layers 30-300hPa (1.53K versus 1.5K) and 300-700hPa (1.28K versus 1.5K). Slightly higher RMS difference for the 700hPa-surface layer (1.78K versus 1.6K) is attributable to land and polar profiles. The AVMP product is within the requirements for 300-600hPa (26.8% versus 35%) and is close in meeting the requirements for 600hPa-surface (25.3% versus 20%). After just one year of maturity, the CrIMSS EDR products are quite comparable to the AIRS heritage algorithm products and show readiness for stages 1-3 validations.
C1 [Divakarla, Murty; Wilson, Michael; Xiong, Xiaozhen; Tan, Changyi; Nalli, Nicholas; Gambacorta, Antonia; Iturbide-Sanchez, Flavio; Sun, Bomin] IM Syst Grp Inc, Rockville, MD 20852 USA.
[Barnet, Christopher] Sci & Technol Corp, Columbia, MD USA.
[Liu, Xu] NASA Langley Res Ctr, Hampton, VA USA.
[Gu, Degui; Hagan, Denise; Ma, Xia-lin] Northrop Grumman Aerosp Syst, Redondo Beach, CA USA.
[Kizer, Susan] Sci Syst & Applicat Inc, Hampton, VA USA.
[Maddy, Eric] Sci & Technol Corp, Hampton, VA 23666 USA.
[Ferraro, Ralph; Reale, Anthony; Goldberg, Mitch] NOAA Ctr Satellite Applicat & Res, College Pk, MD USA.
[Knuteson, Robert] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
[Mollner, Andrew K.] Aerosp Corp, El Segundo, CA 90245 USA.
[Yang, Wenze] Univ Maryland, ESSIC CICS, College Pk, MD 20742 USA.
[Feltz, Michelle] Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI USA.
RP Divakarla, M (reprint author), IM Syst Grp Inc, Rockville, MD 20852 USA.
EM Murty.Divakarla@noaa.gov
RI Reale, Tony/F-5621-2010; Yang, Wenze/B-8356-2012; Sun,
Bomin/P-8742-2014; Gambacorta, Antonia/E-7937-2011; Maddy,
Eric/G-3683-2010; Ferraro, Ralph/F-5587-2010; Nalli,
Nicholas/F-6731-2010; Richards, Amber/K-8203-2015; Divakarla,
Murty/E-7936-2011; Iturbide-Sanchez, Flavio/F-9186-2014; Tan,
Changyi/F-4786-2010; Xiong, Xiaozhen/F-6591-2010; Wilson,
Michael/G-9611-2013
OI Feltz, Michelle/0000-0001-5871-0353; Reale, Tony/0000-0003-2150-5246;
Yang, Wenze/0000-0001-8514-2742; Sun, Bomin/0000-0002-4872-9349;
Gambacorta, Antonia/0000-0002-2446-9132; Maddy,
Eric/0000-0003-1151-339X; Ferraro, Ralph/0000-0002-8393-7135; Nalli,
Nicholas/0000-0002-6914-5537; Divakarla, Murty/0000-0002-0399-3381;
Iturbide-Sanchez, Flavio/0000-0002-8539-0073;
FU JPSS Program Office
FX We wish to thank the European Centre for Medium-Range Forecasting group
and the National Center for Environmental Prediction for providing the
ECMWF and NCEP data used in this paper. We also express our sincere
appreciation to the Jet Propulsion Laboratory and the Goddard Earth
Sciences Data and Information Services Center for providing the AIRS V6
retrievals for the focus days. The funding for this paper has been
provided by the JPSS Program Office and is gratefully acknowledged. The
manuscript contents are solely the opinions of the authors and do not
constitute a statement of policy, decision, or position on behalf of
NOAA, NASA, or the U.S. Government.
NR 51
TC 10
Z9 10
U1 1
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 27
PY 2014
VL 119
IS 8
BP 4953
EP 4977
DI 10.1002/2013JD020438
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AH0KP
UT WOS:000335809100032
ER
PT J
AU Waller, RG
Stone, RP
Johnstone, J
Mondragon, J
AF Waller, Rhian G.
Stone, Robert P.
Johnstone, Julia
Mondragon, Jennifer
TI Sexual Reproduction and Seasonality of the Alaskan Red Tree Coral,
Primnoa pacifica
SO PLOS ONE
LA English
DT Article
ID DEEP-SEA; FUNGIACYATHUS-MARENZELLERI; POCILLOPORA-DAMICORNIS;
FERTILIZATION SUCCESS; MARINE-INVERTEBRATES; WATER CORALS; OCTOCORAL;
ECOLOGY; REEF; GROWTH
AB The red tree coral Primnoa pacifica is an important habitat forming octocoral in North Pacific waters. Given the prominence of this species in shelf and upper slope areas of the Gulf of Alaska where fishing disturbance can be high, it may be able to sustain healthy populations through adaptive reproductive processes. This study was designed to test this hypothesis, examining reproductive mode, seasonality and fecundity in both undamaged and simulated damaged colonies over the course of 16 months using a deepwater-emerged population in Tracy Arm Fjord. Females within the population developed asynchronously, though males showed trends of synchronicity, with production of immature spermatocysts heightened in December/January and maturation of gametes in the fall months. Periodicity of individuals varied from a single year reproductive event to some individuals taking more than the 16 months sampled to produce viable gametes. Multiple stages of gametes occurred in polyps of the same colony during most sampling periods. Mean oocyte size ranged from 50 to 200 mu m in any season, and maximum oocyte size (802 mu m) suggests a lecithotrophic larva. No brooding larvae were found during this study, though unfertilized oocytes were found adhered to the outside of polyps, where they are presumably fertilized. This species demonstrated size-dependent reproduction, with gametes first forming in colonies over 42-cm length, and steady oocyte sizes being achieved after reaching 80-cm in length. The average fecundity was 86 (+/- 12) total oocytes per polyp, and 17 (+/- 12) potential per polyp fecundity. Sub-lethal injury by removing 21-40% of colony tissue had no significant reproductive response in males or females over the course of this study, except for a corresponding loss in overall colony fecundity. The reproductive patterns and long gamete generation times observed in this study indicate that recruitment events are likely to be highly sporadic in this species increasing its vulnerability to anthropogenic disturbances.
C1 [Waller, Rhian G.] Univ Maine, Darling Marine Ctr, Sch Marine Sci, Walpole, ME 04573 USA.
[Stone, Robert P.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK USA.
[Johnstone, Julia] Univ Maine, Darling Marine Ctr, Walpole, ME 04573 USA.
[Mondragon, Jennifer] NOAA, Alaska Reg Off, Natl Marine Fisheries Serv, Juneau, AK USA.
RP Waller, RG (reprint author), Univ Maine, Darling Marine Ctr, Sch Marine Sci, Walpole, ME 04573 USA.
EM rhian.waller@maine.edu
FU National Oceanic and Atmospheric Administration Alaska Fisheries Science
Center; National Geographic Society
FX This work was funded by the National Oceanic and Atmospheric
Administration Alaska Fisheries Science Center, and through the National
Geographic Society. The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 53
TC 7
Z9 8
U1 5
U2 18
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 APR 25
PY 2014
VL 9
IS 4
AR e90893
DI 10.1371/journal.pone.0090893
PG 14
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AI3CM
UT WOS:000336736600001
PM 24770675
ER
PT J
AU Van Gorp, B
Mouroulis, P
Blaney, D
Green, RO
Ehlmann, BL
Rodriguez, JI
AF Van Gorp, Byron
Mouroulis, Pantazis
Blaney, Diana
Green, Robert O.
Ehlmann, Bethany L.
Rodriguez, Jose I.
TI Ultra-compact imaging spectrometer for remote, in situ, and microscopic
planetary mineralogy
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE imaging spectroscopy; imaging spectrometer; mineralogy; Mars rover;
microspectroscopy
ID SPECTROSCOPY; SURFACE
AB The ultra-compact imaging spectrometer is a miniature imaging spectrometer that has been designed for compatibility with operation in a Martian environment. The spectrometer can be mated to a variety of front optics, both telescopic and microscopic. With a miniature telescope, it can serve as a rover mast instrument that surveys the surrounding area from a distance of similar to 1 m to infinity and produces full spectral data (500 to 2500 nm) of a wide panoramic scene in order to find the most mineralogically promising targets for further analysis and for directing subsequent rover activities. With a microscopic front lens, it can serve as an analytical tool for determining types of minerals in a rock and their spatial relations at a scale of tens of micrometers in order to make detailed interpretations of geological history. A realization of the instrument, adapted for operation in the Earth's atmosphere, has been produced and tested both in the laboratory and in the field. The results prove the ability of the instrument to detect and map minerals of interest in both modes of operation. (C) 2014 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Van Gorp, Byron; Mouroulis, Pantazis; Blaney, Diana; Green, Robert O.; Ehlmann, Bethany L.; Rodriguez, Jose I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ehlmann, Bethany L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Van Gorp, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM byron.e.van.gorp@jpl.nasa.gov
NR 21
TC 6
Z9 6
U1 0
U2 5
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 APR 25
PY 2014
VL 8
AR 084988
DI 10.1117/1.JRS.8.084988
PG 16
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AG8BV
UT WOS:000335644600001
ER
PT J
AU Capece, AM
Polk, JE
Mikellides, IG
Shepherd, JE
AF Capece, Angela M.
Polk, James E.
Mikellides, Ioannis G.
Shepherd, Joseph E.
TI Oxygen transport in the internal xenon plasma of a dispenser hollow
cathode
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID IMPREGNATED-CATHODE; ELECTRON-IMPACT; CHARGE-EXCHANGE; CROSS-SECTIONS;
BARIUM; MECHANISM; OPERATION; IONIZATION; BA; ATTACHMENT
AB Reactive gases such as oxygen and water vapor modify the surface morphology of BaO dispenser cathodes and degrade the electron emission properties. For vacuum cathodes operating at fixed temperature, the emission current drops rapidly when oxygen adsorbs on top of the low work function surface. Previous experiments have shown that plasma cathodes are more resistant to oxygen poisoning and can operate with O-2 partial pressures one to two orders of magnitude higher than vacuum cathodes before the onset of poisoning occurs. Plasma cathodes used for electric thrusters are typically operated with xenon; however, gas phase barium, oxygen, and tungsten species may be found in small concentrations. The densities of these minor species are small compared with the plasma density, and thus, their presence in the discharge does not significantly alter the xenon plasma parameters. It is important, however, to consider the transport of these minor species as they may deposit on the emitter surface and affect the electron emission properties. In this work, we present the results of a material transport model used to predict oxygen fluxes to the cathode surface by solving the species conservation equations in a cathode with a 2.25 mm diameter orifice operated at a discharge current of 15 A, a Xe flow rate of 3.7 sccm, and 100 ppm of O-2. The dominant ionization process for O-2 is resonant charge exchange with xenon ions. Ba is effectively recycled in the plasma; however, BaO and O-2 are not. The model shows that the oxygen flux to the surface is not diffusion-limited; therefore, the high resistance to oxygen poisoning observed in plasma cathodes likely results from surface processes not considered here. (C) 2014 AIP Publishing LLC.
C1 [Capece, Angela M.; Shepherd, Joseph E.] CALTECH, Pasadena, CA 91125 USA.
[Polk, James E.; Mikellides, Ioannis G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Capece, AM (reprint author), Princeton Plasma Phys Lab, POB 451, Princeton, NJ 08543 USA.
EM acapece@pppl.gov
RI Shepherd, Joseph/B-5997-2014
OI Shepherd, Joseph/0000-0003-3181-9310
NR 48
TC 1
Z9 1
U1 0
U2 11
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-8979
EI 1089-7550
J9 J APPL PHYS
JI J. Appl. Phys.
PD APR 21
PY 2014
VL 115
IS 15
AR 153302
DI 10.1063/1.4871755
PG 13
WC Physics, Applied
SC Physics
GA AG2DU
UT WOS:000335227100007
ER
PT J
AU Aasi, J
Abadie, J
Abbott, BP
Abbott, R
Abbott, T
Abernathy, MR
Accadia, T
Acernese, F
Adams, C
Adams, T
Adhikari, RX
Affeldt, C
Agathos, M
Aggarwal, N
Aguiar, OD
Ajith, P
Allen, B
Allocca, A
Ceron, EA
Amariutei, D
Anderson, RA
Anderson, SB
Anderson, WG
Arai, K
Araya, MC
Arceneaux, C
Areeda, J
Ast, S
Aston, SM
Astone, P
Aufmuth, P
Aulbert, C
Austin, L
Aylott, BE
Babak, S
Baker, PT
Ballardin, G
Ballmer, SW
Barayoga, JC
Barker, D
Barnum, SH
Barone, F
Barr, B
Barsotti, L
Barsuglia, M
Barton, MA
Bartos, I
Bassiri, R
Basti, A
Batch, J
Bauchrowitz, J
Bauer, TS
Bebronne, M
Behnke, B
Bejger, M
Beker, MG
Bell, AS
Bell, C
Belopolski, I
Bergmann, G
Berliner, JM
Bersanetti, D
Bertolini, A
Bessis, D
Betzwieser, J
Beyersdorf, PT
Bhadbhade, T
Bilenko, IA
Billingsley, G
Birch, J
Bitossi, M
Bizouard, MA
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Blom, M
Bock, O
Bodiya, TP
Boer, M
Bogan, C
Bond, C
Bondu, F
Bonelli, L
Bonnand, R
Bork, R
Born, M
Boschi, V
Bose, S
Bosi, L
Bowers, J
Bradaschia, C
Brady, PR
Braginsky, VB
Branchesi, M
Brannen, CA
Brau, JE
Breyer, J
Briant, T
Bridges, DO
Brillet, A
Brinkmann, M
Brisson, V
Britzger, M
Brooks, AF
Brown, DA
Brown, DD
Bruckner, F
Bulik, T
Bulten, HJ
Buonanno, A
Buskulic, D
Buy, C
Byer, RL
Cadonati, L
Cagnoli, G
Bustillo, JC
Calloni, E
Camp, JB
Campsie, P
Cannon, KC
Canuel, B
Cao, J
Capano, CD
Carbognani, F
Carbone, L
Caride, S
Castiglia, A
Caudill, S
Cavaglia, M
Cavalier, F
Cavalieri, R
Cella, G
Cepeda, C
Cesarini, E
Chakraborty, R
Chalermsongsak, T
Chao, S
Charlton, P
Chassande-Mottin, E
Chen, X
Chen, Y
Chincarini, A
Chiummo, A
Cho, HS
Chow, J
Christensen, N
Chu, Q
Chua, SSY
Chung, S
Ciani, G
Clara, F
Clark, DE
Clark, JA
Cleva, F
Coccia, E
Cohadon, PF
Colla, A
Colombini, M
Constancio, M
Conte, A
Conte, R
Cook, D
Corbitt, TR
Cordier, M
Cornish, N
Corsi, A
Costa, CA
Coughlin, MW
Coulon, JP
Countryman, S
Couvares, P
Coward, DM
Cowart, M
Coyne, DC
Craig, K
Creighton, JDE
Creighton, TD
Crowder, SG
Cumming, A
Cunningham, L
Cuoco, E
Dahl, K
Dal Canton, T
Damjanic, M
Danilishin, SL
D'Antonio, S
Danzmann, K
Dattilo, V
Daudert, B
Daveloza, H
Davier, M
Davies, GS
Daw, EJ
Day, R
Dayanga, T
Debreczeni, G
Degallaix, J
Deleeuw, E
Deleglise, S
Del Pozzo, W
Denker, T
Dent, T
Dereli, H
Dergachev, V
DeRosa, RT
De Rosa, R
DeSalvo, R
Dhurandhar, S
Diaz, M
Dietz, A
Di Fiore, L
Di Lieto, A
Di Palma, I
Di Virgilio, A
Dmitry, K
Donovan, F
Dooley, KL
Doravari, S
Drago, M
Drever, RWP
Driggers, JC
Du, Z
Dumas, JC
Dwyer, S
Eberle, T
Edwards, M
Effler, A
Ehrens, P
Eichholz, J
Eikenberry, SS
EndrHoczi, G
Essick, R
Etzel, T
Evans, K
Evans, M
Evans, T
Factourovich, M
Fafone, V
Fairhurst, S
Fang, Q
Farinon, S
Farr, B
Farr, W
Favata, M
Fazi, D
Fehrmann, H
Feldbaum, D
Ferrante, I
Ferrini, F
Fidecaro, F
Finn, LS
Fiori, I
Fisher, R
Flaminio, R
Foley, E
Foley, S
Forsi, E
Fotopoulos, N
Fournier, JD
Franco, S
Frasca, S
Frasconi, F
Frede, M
Frei, M
Frei, Z
Freise, A
Frey, R
Fricke, TT
Fritschel, P
Frolov, VV
Fujimoto, MK
Fulda, P
Fyffe, M
Gair, J
Gammaitoni, L
Garcia, J
Garufi, F
Gehrels, N
Gemme, G
Genin, E
Gennai, A
Gergely, L
Ghosh, S
Giaime, JA
Giampanis, S
Giardina, KD
Giazotto, A
Gil-Casanova, S
Gill, C
Gleason, J
Goetz, E
Goetz, R
Gondan, L
Gonzalez, G
Gordon, N
Gorodetsky, ML
Gossan, S
Gossler, S
Gouaty, R
Graef, C
Graff, PB
Granata, M
Grant, A
Gras, S
Gray, C
Greenhalgh, RJS
Gretarsson, AM
Griffo, C
Groot, P
Grote, H
Grover, K
Grunewald, S
Guidi, GM
Guido, C
Gushwa, KE
Gustafson, EK
Gustafson, R
Hall, B
Hall, E
Hammer, D
Hammond, G
Hanke, M
Hanks, J
Hanna, C
Hanson, J
Harms, J
Harry, GM
Harry, IW
Harstad, ED
Hartman, MT
Haughian, K
Hayama, K
Heefner, J
Heidmann, A
Heintze, M
Heitmann, H
Hello, P
Hemming, G
Hendry, M
Heng, IS
Heptonstall, AW
Heurs, M
Hild, S
Hoak, D
Hodge, KA
Holt, K
Hong, T
Hooper, S
Horrom, T
Hosken, DJ
Hough, J
Howell, EJ
Hu, Y
Hua, Z
Huang, V
Huerta, EA
Hughey, B
Husa, S
Huttner, SH
Huynh, M
Huynh-Dinh, T
Iafrate, J
Ingram, DR
Inta, R
Isogai, T
Ivanov, A
Iyer, BR
Izumi, K
Jacobson, M
James, E
Jang, H
Jang, YJ
Jaranowski, P
Jimenez-Forteza, F
Johnson, WW
Jones, D
Jones, DI
Jones, R
Jonker, RJG
Ju, L
Haris, K
Kalmus, P
Kalogera, V
Kandhasamy, S
Kang, G
Kanner, JB
Kasprzack, M
Kasturi, R
Katsavounidis, E
Katzman, W
Kaufer, H
Kaufman, K
Kawabe, K
Kawamura, S
Kawazoe, F
Kefelian, F
Keitel, D
Kelley, DB
Kells, W
Keppel, DG
Khalaidovski, A
Khalili, FY
Khazanov, EA
Kim, BK
Kim, C
Kim, K
Kim, N
Kim, W
Kim, YM
King, EJ
King, PJ
Kinzel, DL
Kissel, JS
Klimenko, S
Kline, J
Koehlenbeck, S
Kokeyama, K
Kondrashov, V
Koranda, S
Korth, WZ
Kowalska, I
Kozak, D
Kremin, A
Kringel, V
Krishnan, B
Krolak, A
Kucharczyk, C
Kudla, S
Kuehn, G
Kumar, A
Kumar, P
Kumar, R
Kurdyumov, R
Kwee, P
Landry, M
Lantz, B
Larson, S
Lasky, PD
Lawrie, C
Leaci, P
Lebigot, EO
Lee, CH
Lee, HK
Lee, HM
Lee, J
Lee, J
Leonardi, M
Leong, JR
Le Roux, A
Leroy, N
Letendre, N
Levine, B
Lewis, JB
Lhuillier, V
Li, TGF
Lin, AC
Littenberg, TB
Litvine, V
Liu, F
Liu, H
Liu, Y
Liu, Z
Lloyd, D
Lockerbie, NA
Lockett, V
Lodhia, D
Loew, K
Logue, J
Lombardi, AL
Lorenzini, M
Loriette, V
Lormand, M
Losurdo, G
Lough, J
Luan, J
Lubinski, MJ
Luck, H
Lundgren, AP
Macarthur, J
Macdonald, E
Machenschalk, B
Maclnnis, M
Macleod, DM
Magana-Sandoval, F
Mageswaran, M
Mailand, K
Majorana, E
Maksimovic, I
Malvezzi, V
Man, N
Manca, M
Mandel, I
Mandic, V
Mangano, V
Mantovani, M
Marchesoni, F
Marion, F
Marka, S
Marka, Z
Markosyan, A
Maros, E
Marque, J
Martelli, F
Martin, IW
Martin, RM
Martinelli, L
Martynov, D
Marx, JN
Mason, K
Masserot, A
Massinger, TJ
Matichard, F
Matone, L
Matzner, RA
Mavalvala, N
May, G
Mazumder, N
Mazzolo, G
McCarthy, R
McClelland, DE
McGuire, SC
Mclntyre, G
Mclver, J
Meacher, D
Meadors, GD
Mehmet, M
Meidam, J
Meier, T
Melatos, A
Mendell, G
Mercer, RA
Meshkov, S
Messenger, C
Meyer, MS
Miao, H
Michel, C
Mikhailov, EE
Milano, L
Miller, J
Minenkov, Y
Mingarelli, CMF
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Moe, B
Mohan, M
Mohapatra, SRP
Mokler, F
Moraru, D
Moreno, G
Morgado, N
Mori, T
Morriss, SR
Mossavi, K
Mours, B
Mow-Lowry, CM
Mueller, CL
Mueller, G
Mukherjee, S
Mullavey, A
Munch, J
Murphy, D
Murray, PG
Mytidis, A
Nagy, MF
Kumar, DN
Nardecchia, I
Nash, T
Naticchioni, L
Nayak, R
Necula, V
Nelemans, G
Neri, I
Neri, M
Newton, G
Nguyen, T
Nishida, E
Nishizawa, A
Nitz, A
Nocera, F
Nolting, D
Normandin, ME
Nuttall, LK
Ochsner, E
O'Dell, J
Oelker, E
Ogin, GH
Oh, JJ
Oh, SH
Ohme, F
Oppermann, P
O'Reilly, B
Larcher, WO
O'Shaughnessy, R
Osthelder, C
Ott, CD
Ottaway, DJ
Ottens, RS
Ou, J
Overmier, H
Owen, BJ
Padilla, C
Pai, A
Palomba, C
Pan, Y
Pankow, C
Paoletti, F
Paoletti, R
Papa, MA
Paris, H
Pasqualetti, A
Passaquieti, R
Passuello, D
Pedraza, M
Peiris, P
Penn, S
Perreca, A
Phelps, M
Pichot, M
Pickenpack, M
Piergiovanni, F
Pierro, V
Pinard, L
Pindor, B
Pinto, IM
Pitkin, M
Poeld, J
Poggiani, R
Poole, V
Poux, C
Predoi, V
Prestegard, T
Price, LR
Prijatelj, M
Principe, M
Privitera, S
Prix, R
Prodi, GA
Prokhorov, L
Puncken, O
Punturo, M
Puppo, P
Quetschke, V
Quintero, E
Quitzow-James, R
Raab, FJ
Rabeling, DS
Racz, I
Radkins, H
Raffai, P
Raja, S
Rajalakshmi, G
Rakhmanov, M
Ramet, C
Rapagnani, P
Raymond, V
Re, V
Reed, CM
Reed, T
Regimbau, T
Reid, S
Reitze, DH
Ricci, F
Riesen, R
Riles, K
Robertson, NA
Robinet, F
Rocchi, A
Roddy, S
Rodriguez, C
Rodruck, M
Roever, C
Rolland, L
Rollins, JG
Romano, R
Romanov, G
Romie, JH
Rosinska, D
Rowan, S
Rudiger, A
Ruggi, P
Ryan, K
Salemi, F
Sammut, L
de la Jordana, LS
Sandberg, V
Sanders, J
Sannibale, V
Santiago-Prieto, I
Saracco, E
Sassolas, B
Sathyaprakash, BS
Saulson, PR
Savage, R
Schilling, R
Schnabel, R
Schofield, RMS
Schreiber, E
Schuette, D
Schulz, B
Schutz, BF
Schwinberg, P
Scott, J
Scott, SM
Seifert, F
Sellers, D
Sengupta, AS
Sentenac, D
Sequino, V
Sergeev, A
Shaddock, D
Shah, S
Shahriar, MS
Shaltev, M
Shapiro, B
Shawhan, P
Shoemaker, DH
Sidery, TL
Siellez, K
Siemens, X
Sigg, D
Simakov, D
Singer, A
Singer, L
Sintes, AM
Skelton, GR
Slagmolen, BJJ
Slutsky, J
Smith, JR
Smith, MR
Smith, RJE
Smith-Lefebvre, ND
Soden, K
Son, EJ
Sorazu, B
Souradeep, T
Sperandio, L
Staley, A
Steinert, E
Steinlechner, J
Steinlechner, S
Steplewski, S
Stevens, D
Stochino, A
Stone, R
Strain, KA
Straniero, N
Strigin, S
Stroeer, AS
Sturani, R
Stuver, AL
Summerscales, TZ
Susmithan, S
Sutton, PJ
Swinkels, B
Szeifert, G
Tacca, M
Talukder, D
Tang, L
Tanner, DB
Tarabrin, SP
Taylor, R
ter Braack, APM
Thirugnanasambandam, MP
Thomas, M
Thomas, P
Thorne, KA
Thorne, KS
Thrane, E
Tiwari, V
Tokmakov, KV
Tomlinson, C
Toncelli, A
Tonelli, M
Torre, O
Torres, CV
Torrie, CI
Travasso, F
Traylor, G
Tse, M
Ugolini, D
Unnikrishnan, CS
Vahlbruch, H
Vajente, G
Vallisneri, M
van den Brand, JFJ
Van Den Broeck, C
van der Putten, S
van der Sluys, MV
van Heijningen, J
van Veggel, AA
Vass, S
Vasuth, M
Vaulin, R
Vecchio, A
Vedovato, G
Veitch, J
Veitch, PJ
Venkateswara, K
Verkindt, D
Verma, S
Vetrano, F
Vicere, A
Vincent-Finley, R
Vinet, JY
Vitale, S
Vlcek, B
Vo, T
Vocca, H
Vorvick, C
Vousden, WD
Vrinceanu, D
Vyachanin, SP
Wade, A
Wade, L
Wade, M
Waldman, SJ
Walker, M
Wallace, L
Wan, Y
Wang, J
Wang, M
Wang, X
Wanner, A
Ward, RL
Was, M
Weaver, B
Wei, LW
Weinert, M
Weinstein, AJ
Weiss, R
Welborn, T
Wen, L
Wessels, P
West, M
Westphal, T
Wette, K
Whelan, JT
Whitcomb, SE
White, DJ
Whiting, BF
Wibowo, S
Wiesner, K
Wilkinson, C
Williams, L
Williams, R
Williams, T
Willis, JL
Willke, B
Wimmer, M
Winkelmann, L
Winkler, W
Wipf, CC
Wittel, H
Woan, G
Worden, J
Yablon, J
Yakushin, I
Yamamoto, H
Yancey, CC
Yang, H
Yeaton-Massey, D
Yoshida, S
Yum, H
Yvert, M
Zadrozny, A
Zanolin, M
Zendri, JP
Zhang, F
Zhang, L
Zhao, C
Zhu, H
Zhu, XJ
Zotov, N
Zucker, ME
Zweizig, J
AF Aasi, J.
Abadie, J.
Abbott, B. P.
Abbott, R.
Abbott, T.
Abernathy, M. R.
Accadia, T.
Acernese, F.
Adams, C.
Adams, T.
Adhikari, R. X.
Affeldt, C.
Agathos, M.
Aggarwal, N.
Aguiar, O. D.
Ajith, P.
Allen, B.
Allocca, A.
Ceron, E. Amador
Amariutei, D.
Anderson, R. A.
Anderson, S. B.
Anderson, W. G.
Arai, K.
Araya, M. C.
Arceneaux, C.
Areeda, J.
Ast, S.
Aston, S. M.
Astone, P.
Aufmuth, P.
Aulbert, C.
Austin, L.
Aylott, B. E.
Babak, S.
Baker, P. T.
Ballardin, G.
Ballmer, S. W.
Barayoga, J. C.
Barker, D.
Barnum, S. H.
Barone, F.
Barr, B.
Barsotti, L.
Barsuglia, M.
Barton, M. A.
Bartos, I.
Bassiri, R.
Basti, A.
Batch, J.
Bauchrowitz, J.
Bauer, Th S.
Bebronne, M.
Behnke, B.
Bejger, M.
Beker, M. G.
Bell, A. S.
Bell, C.
Belopolski, I.
Bergmann, G.
Berliner, J. M.
Bersanetti, D.
Bertolini, A.
Bessis, D.
Betzwieser, J.
Beyersdorf, P. T.
Bhadbhade, T.
Bilenko, I. A.
Billingsley, G.
Birch, J.
Bitossi, M.
Bizouard, M. A.
Black, E.
Blackburn, J. K.
Blackburn, L.
Blair, D.
Blom, M.
Bock, O.
Bodiya, T. P.
Boer, M.
Bogan, C.
Bond, C.
Bondu, F.
Bonelli, L.
Bonnand, R.
Bork, R.
Born, M.
Boschi, V.
Bose, S.
Bosi, L.
Bowers, J.
Bradaschia, C.
Brady, P. R.
Braginsky, V. B.
Branchesi, M.
Brannen, C. A.
Brau, J. E.
Breyer, J.
Briant, T.
Bridges, D. O.
Brillet, A.
Brinkmann, M.
Brisson, V.
Britzger, M.
Brooks, A. F.
Brown, D. A.
Brown, D. D.
Brueckner, F.
Bulik, T.
Bulten, H. J.
Buonanno, A.
Buskulic, D.
Buy, C.
Byer, R. L.
Cadonati, L.
Cagnoli, G.
Calderon Bustillo, J.
Calloni, E.
Camp, J. B.
Campsie, P.
Cannon, K. C.
Canuel, B.
Cao, J.
Capano, C. D.
Carbognani, F.
Carbone, L.
Caride, S.
Castiglia, A.
Caudill, S.
Cavaglia, M.
Cavalier, F.
Cavalieri, R.
Cella, G.
Cepeda, C.
Cesarini, E.
Chakraborty, R.
Chalermsongsak, T.
Chao, S.
Charlton, P.
Chassande-Mottin, E.
Chen, X.
Chen, Y.
Chincarini, A.
Chiummo, A.
Cho, H. S.
Chow, J.
Christensen, N.
Chu, Q.
Chua, S. S. Y.
Chung, S.
Ciani, G.
Clara, F.
Clark, D. E.
Clark, J. A.
Cleva, F.
Coccia, E.
Cohadon, P-F
Colla, A.
Colombini, M.
Constancio, M., Jr.
Conte, A.
Conte, R.
Cook, D.
Corbitt, T. R.
Cordier, M.
Cornish, N.
Corsi, A.
Costa, C. A.
Coughlin, M. W.
Coulon, J-P
Countryman, S.
Couvares, P.
Coward, D. M.
Cowart, M.
Coyne, D. C.
Craig, K.
Creighton, J. D. E.
Creighton, T. D.
Crowder, S. G.
Cumming, A.
Cunningham, L.
Cuoco, E.
Dahl, K.
Dal Canton, T.
Damjanic, M.
Danilishin, S. L.
D'Antonio, S.
Danzmann, K.
Dattilo, V.
Daudert, B.
Daveloza, H.
Davier, M.
Davies, G. S.
Daw, E. J.
Day, R.
Dayanga, T.
Debreczeni, G.
Degallaix, J.
Deleeuw, E.
Deleglise, S.
Del Pozzo, W.
Denker, T.
Dent, T.
Dereli, H.
Dergachev, V.
DeRosa, R. T.
De Rosa, R.
DeSalvo, R.
Dhurandhar, S.
Diaz, M.
Dietz, A.
Di Fiore, L.
Di Lieto, A.
Di Palma, I.
Di Virgilio, A.
Dmitry, K.
Donovan, F.
Dooley, K. L.
Doravari, S.
Drago, M.
Drever, R. W. P.
Driggers, J. C.
Du, Z.
Dumas, J-C
Dwyer, S.
Eberle, T.
Edwards, M.
Effler, A.
Ehrens, P.
Eichholz, J.
Eikenberry, S. S.
EndrHoczi, G.
Essick, R.
Etzel, T.
Evans, K.
Evans, M.
Evans, T.
Factourovich, M.
Fafone, V.
Fairhurst, S.
Fang, Q.
Farinon, S.
Farr, B.
Farr, W.
Favata, M.
Fazi, D.
Fehrmann, H.
Feldbaum, D.
Ferrante, I.
Ferrini, F.
Fidecaro, F.
Finn, L. S.
Fiori, I.
Fisher, R.
Flaminio, R.
Foley, E.
Foley, S.
Forsi, E.
Fotopoulos, N.
Fournier, J-D
Franco, S.
Frasca, S.
Frasconi, F.
Frede, M.
Frei, M.
Frei, Z.
Freise, A.
Frey, R.
Fricke, T. T.
Fritschel, P.
Frolov, V. V.
Fujimoto, M-K
Fulda, P.
Fyffe, M.
Gair, J.
Gammaitoni, L.
Garcia, J.
Garufi, F.
Gehrels, N.
Gemme, G.
Genin, E.
Gennai, A.
Gergely, L.
Ghosh, S.
Giaime, J. A.
Giampanis, S.
Giardina, K. D.
Giazotto, A.
Gil-Casanova, S.
Gill, C.
Gleason, J.
Goetz, E.
Goetz, R.
Gondan, L.
Gonzalez, G.
Gordon, N.
Gorodetsky, M. L.
Gossan, S.
Gossler, S.
Gouaty, R.
Graef, C.
Graff, P. B.
Granata, M.
Grant, A.
Gras, S.
Gray, C.
Greenhalgh, R. J. S.
Gretarsson, A. M.
Griffo, C.
Groot, P.
Grote, H.
Grover, K.
Grunewald, S.
Guidi, G. M.
Guido, C.
Gushwa, K. E.
Gustafson, E. K.
Gustafson, R.
Hall, B.
Hall, E.
Hammer, D.
Hammond, G.
Hanke, M.
Hanks, J.
Hanna, C.
Hanson, J.
Harms, J.
Harry, G. M.
Harry, I. W.
Harstad, E. D.
Hartman, M. T.
Haughian, K.
Hayama, K.
Heefner, J.
Heidmann, A.
Heintze, M.
Heitmann, H.
Hello, P.
Hemming, G.
Hendry, M.
Heng, I. S.
Heptonstall, A. W.
Heurs, M.
Hild, S.
Hoak, D.
Hodge, K. A.
Holt, K.
Hong, T.
Hooper, S.
Horrom, T.
Hosken, D. J.
Hough, J.
Howell, E. J.
Hu, Y.
Hua, Z.
Huang, V.
Huerta, E. A.
Hughey, B.
Husa, S.
Huttner, S. H.
Huynh, M.
Huynh-Dinh, T.
Iafrate, J.
Ingram, D. R.
Inta, R.
Isogai, T.
Ivanov, A.
Iyer, B. R.
Izumi, K.
Jacobson, M.
James, E.
Jang, H.
Jang, Y. J.
Jaranowski, P.
Jimenez-Forteza, F.
Johnson, W. W.
Jones, D.
Jones, D. I.
Jones, R.
Jonker, R. J. G.
Ju, L.
Haris, K.
Kalmus, P.
Kalogera, V.
Kandhasamy, S.
Kang, G.
Kanner, J. B.
Kasprzack, M.
Kasturi, R.
Katsavounidis, E.
Katzman, W.
Kaufer, H.
Kaufman, K.
Kawabe, K.
Kawamura, S.
Kawazoe, F.
Kefelian, F.
Keitel, D.
Kelley, D. B.
Kells, W.
Keppel, D. G.
Khalaidovski, A.
Khalili, F. Y.
Khazanov, E. A.
Kim, B. K.
Kim, C.
Kim, K.
Kim, N.
Kim, W.
Kim, Y-M
King, E. J.
King, P. J.
Kinzel, D. L.
Kissel, J. S.
Klimenko, S.
Kline, J.
Koehlenbeck, S.
Kokeyama, K.
Kondrashov, V.
Koranda, S.
Korth, W. Z.
Kowalska, I.
Kozak, D.
Kremin, A.
Kringel, V.
Krishnan, B.
Krolak, A.
Kucharczyk, C.
Kudla, S.
Kuehn, G.
Kumar, A.
Kumar, P.
Kumar, R.
Kurdyumov, R.
Kwee, P.
Landry, M.
Lantz, B.
Larson, S.
Lasky, P. D.
Lawrie, C.
Leaci, P.
Lebigot, E. O.
Lee, C-H
Lee, H. K.
Lee, H. M.
Lee, J.
Lee, J.
Leonardi, M.
Leong, J. R.
Le Roux, A.
Leroy, N.
Letendre, N.
Levine, B.
Lewis, J. B.
Lhuillier, V.
Li, T. G. F.
Lin, A. C.
Littenberg, T. B.
Litvine, V.
Liu, F.
Liu, H.
Liu, Y.
Liu, Z.
Lloyd, D.
Lockerbie, N. A.
Lockett, V.
Lodhia, D.
Loew, K.
Logue, J.
Lombardi, A. L.
Lorenzini, M.
Loriette, V.
Lormand, M.
Losurdo, G.
Lough, J.
Luan, J.
Lubinski, M. J.
Lueck, H.
Lundgren, A. P.
Macarthur, J.
Macdonald, E.
Machenschalk, B.
Maclnnis, M.
Macleod, D. M.
Magana-Sandoval, F.
Mageswaran, M.
Mailand, K.
Majorana, E.
Maksimovic, I.
Malvezzi, V.
Man, N.
Manca, M.
Mandel, I.
Mandic, V.
Mangano, V.
Mantovani, M.
Marchesoni, F.
Marion, F.
Marka, S.
Marka, Z.
Markosyan, A.
Maros, E.
Marque, J.
Martelli, F.
Martin, I. W.
Martin, R. M.
Martinelli, L.
Martynov, D.
Marx, J. N.
Mason, K.
Masserot, A.
Massinger, T. J.
Matichard, F.
Matone, L.
Matzner, R. A.
Mavalvala, N.
May, G.
Mazumder, N.
Mazzolo, G.
McCarthy, R.
McClelland, D. E.
McGuire, S. C.
Mclntyre, G.
Mclver, J.
Meacher, D.
Meadors, G. D.
Mehmet, M.
Meidam, J.
Meier, T.
Melatos, A.
Mendell, G.
Mercer, R. A.
Meshkov, S.
Messenger, C.
Meyer, M. S.
Miao, H.
Michel, C.
Mikhailov, E. E.
Milano, L.
Miller, J.
Minenkov, Y.
Mingarelli, C. M. F.
Mitra, S.
Mitrofanov, V. P.
Mitselmakher, G.
Mittleman, R.
Moe, B.
Mohan, M.
Mohapatra, S. R. P.
Mokler, F.
Moraru, D.
Moreno, G.
Morgado, N.
Mori, T.
Morriss, S. R.
Mossavi, K.
Mours, B.
Mow-Lowry, C. M.
Mueller, C. L.
Mueller, G.
Mukherjee, S.
Mullavey, A.
Munch, J.
Murphy, D.
Murray, P. G.
Mytidis, A.
Nagy, M. F.
Kumar, D. Nanda
Nardecchia, I.
Nash, T.
Naticchioni, L.
Nayak, R.
Necula, V.
Nelemans, G.
Neri, I.
Neri, M.
Newton, G.
Nguyen, T.
Nishida, E.
Nishizawa, A.
Nitz, A.
Nocera, F.
Nolting, D.
Normandin, M. E.
Nuttall, L. K.
Ochsner, E.
O'Dell, J.
Oelker, E.
Ogin, G. H.
Oh, J. J.
Oh, S. H.
Ohme, F.
Oppermann, P.
O'Reilly, B.
Larcher, W. Ortega
O'Shaughnessy, R.
Osthelder, C.
Ott, C. D.
Ottaway, D. J.
Ottens, R. S.
Ou, J.
Overmier, H.
Owen, B. J.
Padilla, C.
Pai, A.
Palomba, C.
Pan, Y.
Pankow, C.
Paoletti, F.
Paoletti, R.
Papa, M. A.
Paris, H.
Pasqualetti, A.
Passaquieti, R.
Passuello, D.
Pedraza, M.
Peiris, P.
Penn, S.
Perreca, A.
Phelps, M.
Pichot, M.
Pickenpack, M.
Piergiovanni, F.
Pierro, V.
Pinard, L.
Pindor, B.
Pinto, I. M.
Pitkin, M.
Poeld, J.
Poggiani, R.
Poole, V.
Poux, C.
Predoi, V.
Prestegard, T.
Price, L. R.
Prijatelj, M.
Principe, M.
Privitera, S.
Prix, R.
Prodi, G. A.
Prokhorov, L.
Puncken, O.
Punturo, M.
Puppo, P.
Quetschke, V.
Quintero, E.
Quitzow-James, R.
Raab, F. J.
Rabeling, D. S.
Racz, I.
Radkins, H.
Raffai, P.
Raja, S.
Rajalakshmi, G.
Rakhmanov, M.
Ramet, C.
Rapagnani, P.
Raymond, V.
Re, V.
Reed, C. M.
Reed, T.
Regimbau, T.
Reid, S.
Reitze, D. H.
Ricci, F.
Riesen, R.
Riles, K.
Robertson, N. A.
Robinet, F.
Rocchi, A.
Roddy, S.
Rodriguez, C.
Rodruck, M.
Roever, C.
Rolland, L.
Rollins, J. G.
Romano, R.
Romanov, G.
Romie, J. H.
Rosinska, D.
Rowan, S.
Ruediger, A.
Ruggi, P.
Ryan, K.
Salemi, F.
Sammut, L.
Sancho de la Jordana, L.
Sandberg, V.
Sanders, J.
Sannibale, V.
Santiago-Prieto, I.
Saracco, E.
Sassolas, B.
Sathyaprakash, B. S.
Saulson, P. R.
Savage, R.
Schilling, R.
Schnabel, R.
Schofield, R. M. S.
Schreiber, E.
Schuette, D.
Schulz, B.
Schutz, B. F.
Schwinberg, P.
Scott, J.
Scott, S. M.
Seifert, F.
Sellers, D.
Sengupta, A. S.
Sentenac, D.
Sequino, V.
Sergeev, A.
Shaddock, D.
Shah, S.
Shahriar, M. S.
Shaltev, M.
Shapiro, B.
Shawhan, P.
Shoemaker, D. H.
Sidery, T. L.
Siellez, K.
Siemens, X.
Sigg, D.
Simakov, D.
Singer, A.
Singer, L.
Sintes, A. M.
Skelton, G. R.
Slagmolen, B. J. J.
Slutsky, J.
Smith, J. R.
Smith, M. R.
Smith, R. J. E.
Smith-Lefebvre, N. D.
Soden, K.
Son, E. J.
Sorazu, B.
Souradeep, T.
Sperandio, L.
Staley, A.
Steinert, E.
Steinlechner, J.
Steinlechner, S.
Steplewski, S.
Stevens, D.
Stochino, A.
Stone, R.
Strain, K. A.
Straniero, N.
Strigin, S.
Stroeer, A. S.
Sturani, R.
Stuver, A. L.
Summerscales, T. Z.
Susmithan, S.
Sutton, P. J.
Swinkels, B.
Szeifert, G.
Tacca, M.
Talukder, D.
Tang, L.
Tanner, D. B.
Tarabrin, S. P.
Taylor, R.
ter Braack, A. P. M.
Thirugnanasambandam, M. P.
Thomas, M.
Thomas, P.
Thorne, K. A.
Thorne, K. S.
Thrane, E.
Tiwari, V.
Tokmakov, K. V.
Tomlinson, C.
Toncelli, A.
Tonelli, M.
Torre, O.
Torres, C. V.
Torrie, C. I.
Travasso, F.
Traylor, G.
Tse, M.
Ugolini, D.
Unnikrishnan, C. S.
Vahlbruch, H.
Vajente, G.
Vallisneri, M.
van den Brand, J. F. J.
Van Den Broeck, C.
van der Putten, S.
van der Sluys, M. V.
van Heijningen, J.
van Veggel, A. A.
Vass, S.
Vasuth, M.
Vaulin, R.
Vecchio, A.
Vedovato, G.
Veitch, J.
Veitch, P. J.
Venkateswara, K.
Verkindt, D.
Verma, S.
Vetrano, F.
Vicere, A.
Vincent-Finley, R.
Vinet, J-Y
Vitale, S.
Vlcek, B.
Vo, T.
Vocca, H.
Vorvick, C.
Vousden, W. D.
Vrinceanu, D.
Vyachanin, S. P.
Wade, A.
Wade, L.
Wade, M.
Waldman, S. J.
Walker, M.
Wallace, L.
Wan, Y.
Wang, J.
Wang, M.
Wang, X.
Wanner, A.
Ward, R. L.
Was, M.
Weaver, B.
Wei, L-W
Weinert, M.
Weinstein, A. J.
Weiss, R.
Welborn, T.
Wen, L.
Wessels, P.
West, M.
Westphal, T.
Wette, K.
Whelan, J. T.
Whitcomb, S. E.
White, D. J.
Whiting, B. F.
Wibowo, S.
Wiesner, K.
Wilkinson, C.
Williams, L.
Williams, R.
Williams, T.
Willis, J. L.
Willke, B.
Wimmer, M.
Winkelmann, L.
Winkler, W.
Wipf, C. C.
Wittel, H.
Woan, G.
Worden, J.
Yablon, J.
Yakushin, I.
Yamamoto, H.
Yancey, C. C.
Yang, H.
Yeaton-Massey, D.
Yoshida, S.
Yum, H.
Yvert, M.
Zadrozny, A.
Zanolin, M.
Zendri, J-P
Zhang, F.
Zhang, L.
Zhao, C.
Zhu, H.
Zhu, X. J.
Zotov, N.
Zucker, M. E.
Zweizig, J.
TI Application of a Hough search for continuous gravitational waves on data
from the fifth LIGO science run
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
DE gravitational waves; LIGO; neutron stars
ID SPIN-DOWN LIMIT; PERIODIC SOURCES; EMISSION; PULSAR; RADIATION
AB We report on an all-sky search for periodic gravitational waves in the frequency range 50-1000 Hz with the first derivative of frequency in the range -8.9 Chi 10(-10) Hz s(-1) to zero in two years of data collected during LIGO's fifth science run. Our results employ a Hough transform technique, introducing a chi(2) test and analysis of coincidences between the signal levels in years 1 and 2 of observations that offers a significant improvement in the product of strain sensitivity with compute cycles per data sample compared to previously published searches. Since our search yields no surviving candidates, we present results taking the form of frequency dependent, 95% confidence upper limits on the strain amplitude h(0). The most stringent upper limit from year 1 is 1.0 Chi 10(-24) in the 158.00-158.25 Hz band. In year 2, the most stringent upper limit is 8.9 Chi 10(-25) in the 146.50-146.75 Hz band. This improved detection pipeline, which is computationally efficient by at least two orders of magnitude better than our flagship Einstein@ Home search, will be important for 'quicklook' searches in the Advanced LIGO and Virgo detector era.
C1 [Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Ajith, P.; Anderson, R. A.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chakraborty, R.; Chalermsongsak, T.; Coyne, D. C.; Daudert, B.; Dergachev, V.; Driggers, J. C.; Ehrens, P.; Etzel, T.; Fotopoulos, N.; Gushwa, K. E.; Gustafson, E. K.; Hall, E.; Harms, J.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D.; Lewis, J. B.; Litvine, V.; Lloyd, D.; Mageswaran, M.; Mailand, K.; Maros, E.; Martynov, D.; Marx, J. N.; Mclntyre, G.; Meshkov, S.; Nash, T.; Ogin, G. H.; Osthelder, C.; Pedraza, M.; Phelps, M.; Poux, C.; Price, L. R.; Privitera, S.; Quintero, E.; Raymond, V.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Seifert, F.; Singer, A.; Singer, L.; Smith, M. R.; Smith-Lefebvre, N. D.; Taylor, R.; Thirugnanasambandam, M. P.; Thrane, E.; Torrie, C. I.; Vass, S.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Williams, R.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Abbott, T.; Bowers, J.; Corbitt, T. R.; DeRosa, R. T.; Effler, A.; Giaime, J. A.; Gonzalez, G.; Iafrate, J.; Johnson, W. W.; Kokeyama, K.; Kudla, S.; May, G.; Mullavey, A.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Accadia, T.; Bebronne, M.; Buskulic, D.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Verkindt, D.; Yvert, M.] Univ Savoie, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules LAPP, F-74941 Annecy Le Vieux, France.
[Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Garufi, F.; Milano, L.; Romano, R.] Ist Nazl Fis Nucl, Sez Napoli, 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.; Doravari, S.; Evans, T.; Feldbaum, D.; Forsi, E.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Guido, C.; Hanson, J.; Heintze, M.; 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.; Thomas, M.; Thorne, K. A.; Traylor, G.; Welborn, T.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA.
[Adams, T.; Edwards, M.; Fairhurst, S.; Liu, H.; Macdonald, E.; Macleod, D. M.; Nuttall, L. K.; Ohme, F.; Predoi, V.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Affeldt, C.; Allen, B.; Aulbert, C.; Bauchrowitz, J.; Bergmann, G.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Dal Canton, T.; Damjanic, M.; Danzmann, K.; Denker, T.; Dent, T.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Goetz, E.; Gossler, S.; Grote, H.; Hanke, M.; Heurs, M.; Kawazoe, F.; Keitel, D.; Keppel, D. G.; Khalaidovski, A.; Koehlenbeck, S.; Kringel, V.; Krishnan, B.; Kuehn, G.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Manca, M.; Mazzolo, G.; Mehmet, M.; Mokler, F.; Mossavi, K.; Mow-Lowry, C. M.; Oppermann, P.; Pickenpack, M.; Poeld, J.; Prijatelj, M.; Prix, R.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schreiber, E.; Schuette, D.; Schulz, B.; Shaltev, M.; Simakov, D.; Slutsky, J.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Wanner, A.; Was, M.; 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.
[Agathos, M.; Bauer, Th S.; Beker, M. G.; Bertolini, A.; Blom, M.; Bulten, H. J.; Del Pozzo, W.; Jonker, R. J. G.; Li, T. G. F.; Meidam, J.; Nelemans, G.; Rabeling, D. S.; Shah, S.; ter Braack, A. P. M.; van den Brand, J. F. J.; Van Den Broeck, C.; van der Putten, S.; van der Sluys, M. V.; van Heijningen, J.; Veitch, J.; Vitale, S.] Nikhef, NL-1098 XG Amsterdam, Netherlands.
[Aggarwal, N.; Barnum, S. H.; Barsotti, L.; Bodiya, T. P.; Donovan, F.; Essick, R.; Evans, M.; Foley, S.; Fritschel, P.; Gras, S.; Isogai, T.; Katsavounidis, E.; Kissel, J. S.; Kwee, P.; Lee, J.; Maclnnis, M.; Mason, K.; Matichard, F.; Mavalvala, N.; Mittleman, R.; Oelker, E.; Shoemaker, D. H.; Vaulin, R.; Vitale, S.; Waldman, S. J.; Weiss, R.; Wipf, C. C.; Zhang, F.; Zucker, M. E.] MIT, LIGO, Cambridge, MA 02139 USA.
[Aguiar, O. D.; Constancio, M., Jr.; Costa, C. A.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Allen, B.; Ceron, E. Amador; Anderson, W. G.; Brady, P. R.; Caudill, S.; Creighton, J. D. E.; Giampanis, S.; Hammer, D.; Huynh, M.; Kline, J.; Koranda, S.; Mercer, R. A.; Moe, B.; Ochsner, E.; O'Shaughnessy, R.; Pankow, C.; Papa, M. A.; Siemens, X.; Skelton, G. R.; Soden, K.; Vlcek, B.; Wade, L.; Wade, M.; Wibowo, S.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Allen, B.; Ast, S.; Aufmuth, P.; Danzmann, K.; Kaufer, H.; Lueck, H.; Meier, T.; Schnabel, R.; Vahlbruch, H.; Willke, B.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Allocca, A.; Basti, A.; Bitossi, M.; Bonelli, L.; Boschi, V.; Bradaschia, C.; Cella, G.; 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.
[Allocca, A.; Paoletti, R.; Torre, O.] Univ Siena, I-53100 Siena, Italy.
[Amariutei, D.; Ciani, G.; Deleeuw, E.; Eichholz, J.; Eikenberry, S. S.; Feldbaum, D.; Fulda, P.; Gleason, J.; Goetz, R.; Hartman, M. T.; Heintze, M.; Klimenko, S.; Liu, Z.; Martin, R. M.; Mitselmakher, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Kumar, D. Nanda; Necula, V.; Ottens, R. S.; Reitze, D. H.; Tanner, D. B.; Tiwari, V.; Whiting, B. F.; Williams, L.] Univ Florida, Gainesville, FL 32611 USA.
[Arceneaux, C.; Cavaglia, M.; Dietz, A.] Univ Mississippi, University, MS 38677 USA.
[Areeda, J.; Foley, E.; Griffo, C.; Lee, J.; Lockett, V.; Magana-Sandoval, F.; Padilla, C.; Smith, J. R.] Calif State Univ Fullerton, Fullerton, CA 92831 USA.
[Astone, P.; Colla, A.; Conte, A.; Frasca, S.; Majorana, E.; Mangano, V.; Naticchioni, L.; Palomba, C.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
[Aylott, B. E.; Bond, C.; Brown, D. D.; Brueckner, F.; Carbone, L.; Freise, A.; Grover, K.; Lodhia, D.; Mandel, I.; Mingarelli, C. M. F.; Sidery, T. L.; Smith, R. J. E.; Vecchio, A.; Vousden, W. D.; Wang, M.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Babak, S.; Behnke, B.; Grunewald, S.; Leaci, P.; Papa, M. A.; Schutz, B. F.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Baker, P. T.; Cornish, N.] Montana State Univ, Bozeman, MT 59717 USA.
[Ballardin, G.; Canuel, B.; Carbognani, F.; Cavalieri, R.; Chiummo, A.; Cuoco, E.; Dattilo, V.; Day, R.; 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.] European Gravitat Observ, I-56021 Pisa, Italy.
[Ballmer, S. W.; Brown, D. A.; Couvares, P.; Fisher, R.; Harry, I. W.; Huerta, E. A.; Kelley, D. B.; Kumar, P.; Lough, J.; Massinger, T. J.; Mohapatra, S. R. P.; Nitz, A.; Perreca, A.; Saulson, P. R.; West, M.] Syracuse Univ, Syracuse, NY 13244 USA.
[Barker, D.; Barton, M. A.; Batch, J.; Berliner, J. M.; Clara, F.; Cook, D.; Dwyer, S.; Garcia, J.; Gray, C.; Hanks, J.; Ingram, D. R.; Izumi, K.; Jones, D.; Kawabe, K.; Landry, M.; Levine, B.; Lhuillier, V.; Lubinski, M. J.; McCarthy, R.; Mendell, G.; Moraru, D.; Moreno, G.; Paris, H.; Raab, F. J.; Radkins, H.; Reed, C. M.; Rodruck, M.; Ryan, K.; Sandberg, V.; Savage, R.; Schwinberg, P.; Sigg, D.; Steinert, E.; Thomas, P.; Vo, T.; Vorvick, C.; Weaver, B.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA.
[Barr, B.; Bassiri, R.; Bell, A. S.; Bell, C.; Campsie, P.; Craig, K.; Cunningham, L.; Davies, G. S.; Evans, K.; Gill, C.; Gordon, N.; Grant, A.; Hammond, G.; Haughian, K.; Hendry, M.; Heng, I. S.; Hild, S.; Hough, J.; Hu, Y.; Huttner, S. H.; Jones, R.; Kumar, R.; Lawrie, C.; Logue, J.; Macarthur, J.; Martin, I. W.; Messenger, C.; Murray, P. G.; Newton, G.; Pitkin, M.; Robertson, N. A.; Rowan, S.; Santiago-Prieto, I.; Scott, J.; Sorazu, B.; Strain, K. A.; Torrie, C. I.; van Veggel, A. A.; Woan, G.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Barsuglia, M.; Buy, C.; Chassande-Mottin, E.; Tacca, M.] Univ Paris Diderot, Observ Paris, CNRS IN2P3, Sorbonne Paris Cite,CEA Irfu,APC, F-75205 Paris 13, France.
[Bartos, I.; Belopolski, I.; Countryman, S.; Factourovich, M.; Marka, S.; Marka, Z.; Matone, L.; Murphy, D.; Raffai, P.; Staley, A.; Tse, M.] Columbia Univ, New York, NY 10027 USA.
[Bassiri, R.; Bhadbhade, T.; Byer, R. L.; Clark, D. E.; Kim, N.; Kucharczyk, C.; Kurdyumov, R.; Lantz, B.; Lin, A. C.; Markosyan, A.; Shapiro, B.] Stanford Univ, Stanford, CA 94305 USA.
[Basti, A.; Bonelli, L.; Di Lieto, A.; Ferrante, I.; Fidecaro, F.; Passaquieti, R.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Vajente, G.] Univ Pisa, I-56127 Pisa, Italy.
[Bejger, M.; Rosinska, D.] CAMK PAN, PL-00716 Warsaw, Poland.
[Bersanetti, D.; Chincarini, A.; Farinon, S.; Gemme, G.; Neri, M.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy.
[Bersanetti, D.; Neri, M.] Univ Genoa, I-16146 Genoa, Italy.
[Bessis, D.; Creighton, T. D.; Daveloza, H.; Diaz, M.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E.; Larcher, W. Ortega; Puncken, O.; Quetschke, V.; Rakhmanov, M.; Stone, R.; Stroeer, A. S.; Tang, L.; Torres, C. V.; Vrinceanu, D.] 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.; Dmitry, K.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L.; Strigin, S.; Vyachanin, 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.] Univ Paris 11, CNRS, IN2P3, LAL, F-91898 Orsay, France.
[Blackburn, J. K.; Camp, J. B.; Gehrels, N.; Graff, P. B.; Kanner, J. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blair, D.; Chen, X.; Chu, Q.; Chung, S.; Coward, D. M.; Danilishin, S. L.; Dumas, J-C; Fang, Q.; Hooper, S.; Howell, E. J.; Ju, L.; Susmithan, S.; Verma, S.; Wen, L.; Whitcomb, S. E.; Zhao, C.; Zhu, X. J.] Univ Western Australia, Crawley, WA 6009, Australia.
[Boer, M.; Brillet, A.; Cleva, F.; Coulon, J-P; Dereli, H.; Fournier, J-D; Heitmann, H.; Kefelian, F.; Man, N.; Martinelli, L.; Meacher, D.; Pichot, M.; Regimbau, T.; Siellez, K.; Vinet, J-Y; Wei, L-W] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice, France.
[Bondu, F.] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France.
[Bonnand, R.; Cagnoli, G.; Degallaix, J.; Flaminio, R.; Granata, M.; Michel, C.; Morgado, N.; Pinard, L.; Saracco, E.; Sassolas, B.; Straniero, N.] Univ Lyon, CNRS, IN2P3, Lab Mat Avances, F-69622 Lyon, France.
[Bose, S.; Brannen, C. A.; Dayanga, T.; Ghosh, S.; Hall, B.; Poole, V.; Steplewski, S.] Washington State Univ, Pullman, WA 99164 USA.
[Bosi, L.; Colombini, M.; Gammaitoni, L.; Marchesoni, F.; Neri, I.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Branchesi, M.; Guidi, G. M.; Losurdo, G.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Florence, Italy.
[Branchesi, M.; Guidi, G. M.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Univ Urbino Carlo Bo, I-61029 Urbino, Italy.
[Brau, J. E.; Frey, R.; Harstad, E. D.; Quitzow-James, R.; Schofield, R. M. S.; Talukder, D.] Univ Oregon, Eugene, OR 97403 USA.
[Briant, T.; Cohadon, P-F; Deleglise, S.; Heidmann, A.] Univ Paris 06, CNRS, ENS, Lab Kastler Brossel, F-75005 Paris, France.
[Bulik, T.; Kowalska, I.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
[Bulten, H. J.; Rabeling, D. S.; van den Brand, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands.
[Buonanno, A.; Capano, C. D.; Pan, Y.; Shawhan, P.; Yancey, C. C.] Univ Maryland, College Pk, MD 20742 USA.
[Cadonati, L.; Clark, J. A.; Hoak, D.; Lombardi, A. L.; Mclver, J.] Univ Massachusetts, Amherst, MA 01003 USA.
[Calderon Bustillo, J.; Gil-Casanova, S.; Husa, S.; Jimenez-Forteza, F.; Sancho de la Jordana, L.; Sintes, A. M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain.
[Calloni, E.; De Rosa, R.; Garufi, F.; Milano, L.] Univ Naples Federico II, I-80126 Naples, Italy.
[Cannon, K. C.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Cao, J.; Du, Z.; Hua, Z.; Lebigot, E. O.; Liu, Y.; Wan, Y.; Wang, X.] Tsinghua Univ, Beijing 100084, Peoples R China.
[Caride, S.; Gustafson, R.; Meadors, G. D.; Riles, K.; Sanders, J.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Castiglia, A.; Frei, M.; Mohapatra, S. R. P.; Peiris, P.; Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Cesarini, E.; D'Antonio, S.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Minenkov, Y.; Nardecchia, I.; Re, V.; Rocchi, A.; Sequino, V.; Sperandio, L.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Chao, S.; Huang, V.; Ou, J.; Wang, J.] Natl Tsing Hua Univ, Hsinchu 300, Taiwan.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Chen, Y.; Gossan, S.; Hong, T.; Kaufman, K.; Luan, J.; Miao, H.; Ott, C. D.; Thorne, K. S.; Vallisneri, M.; Yang, H.] Caltech CaRT, Pasadena, CA 91125 USA.
[Cho, H. S.; Kim, Y-M; Lee, C-H] Pusan Natl Univ, Pusan 609735, South Korea.
[Chow, J.; Chua, S. S. Y.; Inta, R.; McClelland, D. E.; Miller, J.; Nguyen, T.; Scott, S. M.; Shaddock, D.; Slagmolen, B. J. J.; Stochino, A.; Wade, A.; Ward, R. L.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Christensen, N.] Carleton Coll, Northfield, MN 55057 USA.
[Coccia, E.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy.
[Coccia, E.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Nardecchia, I.; Re, V.; Sequino, V.; Sperandio, L.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Colla, A.; Conte, A.; Frasca, S.; Mangano, V.; Naticchioni, L.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Conte, R.; DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[Conte, R.; DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Corsi, A.] George Washington Univ, Washington, DC 20052 USA.
[Coughlin, M. W.; Gair, J.] Univ Cambridge, Cambridge CB2 1TN, England.
[Crowder, S. G.; Kandhasamy, S.; Kremin, A.; Mandic, V.; Prestegard, T.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Daw, E. J.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[Debreczeni, G.; EndrHoczi, G.; Nagy, M. F.; Racz, I.; Vasuth, M.] Wigner RCP, RMKI, H-1121 Budapest, Hungary.
[Dhurandhar, S.; Mitra, S.; Souradeep, T.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Drago, M.; Leonardi, M.; Prodi, G. A.] Ist Nazl Fis Nucl, Grp Collegato Trento, I-38050 Povo, Trento, Italy.
[Drago, M.; Leonardi, M.; Prodi, G. A.] Univ Trento, I-38050 Povo, Trento, Italy.
[Drever, R. W. P.] CALTECH, Pasadena, CA 91125 USA.
[Farr, B.; Farr, W.; Fazi, D.; Jang, Y. J.; Kalogera, V.; Littenberg, T. B.; Rodriguez, C.; Shahriar, M. S.; Stevens, D.; Yablon, J.; Yum, H.] Northwestern Univ, Evanston, IL 60208 USA.
[Favata, M.] Montclair State Univ, Montclair, NJ 07043 USA.
[Finn, L. S.; Owen, B. J.; Zhu, H.] Penn State Univ, University Pk, PA 16802 USA.
[Frei, Z.; Gergely, L.; Gondan, L.; Raffai, P.; Szeifert, G.] MTA Eotvos Univ, Lendulet ARG, H-1117 Budapest, Hungary.
[Fujimoto, M-K; Hayama, K.; Kawamura, S.; Mori, T.; Nishida, E.; Nishizawa, A.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Gammaitoni, L.; Neri, I.; Travasso, F.; Vocca, H.] Univ Perugia, I-06123 Perugia, Italy.
[Greenhalgh, R. J. S.; O'Dell, J.] HSIC, Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Gretarsson, A. M.; Hughey, B.; Loew, K.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Groot, P.; Nelemans, G.; Shah, S.; van der Sluys, M. V.] Radboud Univ Nijmegen, Dept Astrophy IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Hanna, C.] Perimeter Inst Theoret Phys, Toronto, ON N2L 2Y5, Canada.
[Harry, G. M.] Amer Univ, Washington, DC 20016 USA.
[Horrom, T.; Mikhailov, E. E.; Romanov, G.] Coll William & Mary, Williamsburg, VA 23187 USA.
[Hosken, D. J.; Kim, W.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Iyer, B. R.] Raman Res Inst, Bangalore 560080, Karnataka, India.
[Jang, H.; Kang, G.; Kim, B. K.; Kim, C.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea.
[Jaranowski, P.] Bialystok Univ, PL-15424 Bialystok, Poland.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Haris, K.; Mazumder, N.; Pai, A.] IISER TVM, Trivandrum 695016, Kerala, India.
[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.; Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Krolak, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Kumar, A.] Inst Plasma Res, Bhat 382428, Gandhinagar, India.
[Larson, S.] Utah State Univ, Logan, UT 84322 USA.
[Lasky, P. D.; Melatos, A.; Pindor, B.; Sammut, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
[Liu, F.] Univ Brussels, B-1050 Brussels, Belgium.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy.
[Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA.
[McGuire, S. C.; Vincent-Finley, R.] Southern Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.; Vincent-Finley, R.] A&M Coll, Baton Rouge, LA 70813 USA.
[Nayak, R.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Taejon 305390, South Korea.
[Raja, S.] RRCAT, Indore 452013, Madhya Pradesh, India.
[Rajalakshmi, G.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
[Reid, S.] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland.
[Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
[Sengupta, A. S.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Vedovato, G.; Zendri, J-P] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Williams, T.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
[Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
EM alicia.sintes@uib.es
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Gianluca/0000-0002-3061-9870
FU United States National Science Foundation; Science and Technology
Facilities Council of the United Kingdom; Max-Planck-Society; State of
Niedersachsen/Germany; 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; Netherlands Organisation for Scientific
Research; Polish Ministry of Science and Higher Education; Foundation
for Polish Science; Royal Society; Scottish Funding Council; Scottish
Universities Physics Alliance; National Aeronautics and Space
Administration; Carnegie Trust; Leverhulme Trust; David and Lucile
Packard Foundation; 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 Carnegie Trust, the Leverhulme
Trust, the David and Lucile Packard Foundation, the Research
Corporation, and the Alfred P Sloan Foundation. This document has been
assigned LIGO Laboratory document number LIGO- P1300071.
NR 41
TC 9
Z9 9
U1 9
U2 50
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
EI 1361-6382
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD APR 21
PY 2014
VL 31
IS 8
AR 085014
DI 10.1088/0264-9381/31/8/085014
PG 35
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA AF0QK
UT WOS:000334418900015
ER
PT J
AU Aasi, J
Abadie, J
Abbott, BP
Abbott, R
Abbott, T
Abernathy, MR
Accadia, T
Acernese, F
Adams, C
Adams, T
Adhikari, RX
Affeldt, C
Agathos, M
Aggarwal, N
Aguiar, OD
Ajith, P
Allen, B
Allocca, A
Ceron, EA
Amariutei, D
Anderson, RA
Anderson, SB
Anderson, WG
Arai, K
Araya, MC
Arceneaux, C
Areeda, J
Ast, S
Aston, SM
Astone, P
Aufmuth, P
Aulbert, C
Austin, L
Aylott, BE
Babak, S
Baker, PT
Ballardin, G
Ballmer, SW
Barayoga, JC
Barker, D
Barnum, SH
Barone, F
Barr, B
Barsotti, L
Barsuglia, M
Barton, MA
Bartos, I
Bassiri, R
Basti, A
Batch, J
Bauchrowitz, J
Bauer, TS
Bebronne, M
Behnke, B
Bejger, M
Beker, MG
Bell, AS
Bell, C
Belopolski, I
Bergmann, G
Berliner, JM
Bersanetti, D
Bertolini, A
Bessis, D
Betzwieser, J
Beyersdorf, PT
Bhadbhade, T
Bilenko, IA
Billingsley, G
Birch, J
Bitossi, M
Bizouard, MA
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Blom, M
Bock, O
Bodiya, TP
Boer, M
Bogan, C
Bond, C
Bondu, F
Bonelli, L
Bonnand, R
Bork, R
Born, M
Boschi, V
Bose, S
Bosi, L
Bowers, J
Bradaschia, C
Brady, PR
Braginsky, VB
Branchesi, M
Brannen, CA
Brau, JE
Breyer, J
Briant, T
Bridges, DO
Brillet, A
Brinkmann, M
Brisson, V
Britzger, M
Brooks, AF
Brown, DA
Brown, DD
Brueckner, F
Bulik, T
Bulten, HJ
Buonanno, A
Buskulic, D
Buy, C
Byer, RL
Cadonati, L
Cagnoli, G
Bustillo, JC
Calloni, E
Camp, JB
Campsie, P
Cannon, KC
Canuel, B
Cao, J
Capano, CD
Carbognani, F
Carbone, L
Caride, S
Castiglia, A
Caudill, S
Cavaglia, M
Cavalier, F
Cavalieri, R
Cella, G
Cepeda, C
Cesarini, E
Chakraborty, R
Chalermsongsak, T
Chao, S
Charlton, P
Chassande-Mottin, E
Chen, X
Chen, Y
Chincarini, A
Chiummo, A
Cho, HS
Chow, J
Christensen, N
Chu, Q
Chua, SSY
Chung, S
Ciani, G
Clara, F
Clark, DE
Clark, JA
Cleva, F
Coccia, E
Cohadon, PF
Colla, A
Colombini, M
Jr, MC
Conte, A
Conte, R
Cook, D
Corbitt, TR
Cordier, M
Cornish, N
Corsi, A
Costa, CA
Coughlin, MW
Coulon, JP
Countryman, S
Couvares, P
Coward, DM
Cowart, M
Coyne, DC
Craig, K
Creighton, JDE
Creighton, TD
Crowder, SG
Cumming, A
Cunningham, L
Cuoco, E
Dahl, K
Dal Canton, T
Damjanic, M
Danilishin, SL
D'Antonio, S
Danzmann, K
Dattilo, V
Daudert, B
Daveloza, H
Davier, M
Davies, GS
Daw, EJ
Day, R
Dayanga, T
De Rosa, R
Debreczeni, G
Degallaix, J
Del Pozzo, W
Deleeuw, E
Deleglise, S
Denker, T
Dent, T
Dereli, H
Dergachev, V
DeRosa, R
DeSalvo, R
Dhurandhar, S
Di Fiore, L
Di Lieto, A
Di Palma, I
Di Virgilio, A
Diaz, M
Dietz, A
Dmitry, K
Donovan, F
Dooley, KL
Doravari, S
Drago, M
Drever, RWP
Driggers, JC
Du, Z
Dumas, JC
Dwyer, S
Eberle, T
Edwards, M
Effler, A
Ehrens, P
Eichholz, J
Eikenberry, SS
Endroczi, G
Essick, R
Etzel, T
Evans, K
Evans, M
Evans, T
Factourovich, M
Fafone, V
Fairhurst, S
Fang, Q
Farinon, S
Farr, B
Farr, W
Favata, M
Fazi, D
Fehrmann, H
Feldbaum, D
Ferrante, I
Ferrini, F
Fidecaro, F
Finn, LS
Fiori, I
Fisher, R
Flaminio, R
Foley, E
Foley, S
Forsi, E
Fotopoulos, N
Fournier, JD
Franco, S
Frasca, S
Frasconi, F
Frede, M
Frei, M
Frei, Z
Freise, A
Frey, R
Fricke, TT
Fritschel, P
Frolov, VV
Fujimoto, MK
Fulda, P
Fyffe, M
Gair, J
Gammaitoni, L
Garcia, J
Garufi, F
Gehrels, N
Gemme, G
Genin, E
Gennai, A
Gergely, L
Ghosh, S
Giaime, JA
Giampanis, S
Giardina, KD
Giazotto, A
Gil-Casanova, S
Gill, C
Gleason, J
Goetz, E
Goetz, R
Gondan, L
Gonzalez, G
Gordon, N
Gorodetsky, ML
Gossan, S
Gossler, S
Gouaty, R
Graef, C
Graff, PB
Granata, M
Grant, A
Gras, S
Gray, C
Greenhalgh, RJS
Gretarsson, AM
Griffo, C
Groot, P
Grote, H
Grover, K
Grunewald, S
Guidi, GM
Guido, C
Gushwa, KE
Gustafson, EK
Gustafson, R
Hall, B
Hall, E
Hammer, D
Hammond, G
Hanke, M
Hanks, J
Hanna, C
Hanson, J
Harms, J
Harry, GM
Harry, IW
Harstad, ED
Hartman, MT
Haughian, K
Hayama, K
Heefner, J
Heidmann, A
Heintze, M
Heitmann, H
Hello, P
Hemming, G
Hendry, M
Heng, IS
Heptonstall, AW
Heurs, M
Hild, S
Hoak, D
Hodge, KA
Holt, K
Holtrop, M
Hong, T
Hooper, S
Horrom, T
Hosken, DJ
Hough, J
Howell, EJ
Hu, Y
Hua, Z
Huang, V
Huerta, EA
Hughey, B
Husa, S
Huttner, SH
Huynh, M
Huynh-Dinh, T
Iafrate, J
Ingram, DR
Inta, R
Isogai, T
Ivanov, A
Iyer, BR
Izumi, K
Jacobson, M
James, E
Jang, H
Jang, YJ
Jaranowski, P
Jimenez-Forteza, F
Johnson, WW
Jones, D
Jones, DI
Jones, R
Jonker, RJG
Ju, L
Haris, K
Kalmus, P
Kalogera, V
Kandhasamy, S
Kang, G
Kanner, JB
Kasprzack, M
Kasturi, R
Katsavounidis, E
Katzman, W
Kaufer, H
Kaufman, K
Kawabe, K
Kawamura, S
Kawazoe, F
Kefelian, F
Keitel, D
Kelley, DB
Kells, W
Keppel, DG
Khalaidovski, A
Khalili, FY
Khazanov, EA
Kim, BK
Kim, C
Kim, K
Kim, N
Kim, W
Kim, YM
King, EJ
King, PJ
Kinzel, DL
Kissel, JS
Klimenko, S
Kline, J
Koehlenbeck, S
Kokeyama, K
Kondrashov, V
Koranda, S
Korth, WZ
Kowalska, I
Kozak, D
Kremin, A
Kringel, V
Krishnan, B
Krolak, A
Kucharczyk, C
Kudla, S
Kuehn, G
Kumar, A
Kumar, P
Kumar, R
Kurdyumov, R
Kwee, P
Landry, M
Lantz, B
Larson, S
Lasky, PD
Lawrie, C
Lazzarini, A
Le Roux, A
Leaci, P
Lebigot, EO
Lee, CH
Lee, HK
Lee, HM
Lee, J
Lee, J
Leonardi, M
Leong, JR
Leroy, N
Letendre, N
Levine, B
Lewis, JB
Lhuillier, V
Li, TGF
Lin, AC
Littenberg, TB
Litvine, V
Liu, F
Liu, H
Liu, Y
Liu, Z
Lloyd, D
Lockerbie, NA
Lockett, V
Lodhia, D
Loew, K
Logue, J
Lombardi, AL
Lorenzini, M
Loriette, V
Lormand, M
Losurdo, G
Lough, J
Luan, J
Lubinski, MJ
Lueck, H
Lundgren, AP
Macarthur, J
Macdonald, E
Machenschalk, B
MacInnis, M
Macleod, DM
Magana-Sandoval, F
Mageswaran, M
Mailand, K
Majorana, E
Maksimovic, I
Malvezzi, V
Man, N
Manca, GM
Mandel, I
Mandic, V
Mangano, V
Mantovani, M
Marchesoni, F
Marion, F
Marka, S
Marka, Z
Markosyan, A
Maros, E
Marque, J
Martelli, F
Martin, IW
Martin, RM
Martinelli, L
Martynov, D
Marx, JN
Mason, K
Masserot, A
Massinger, TJ
Matichard, F
Matone, L
Matzner, RA
Mavalvala, N
May, G
Mazumder, N
Mazzolo, G
McCarthy, R
McClelland, DE
McGuire, SC
McIntyre, G
McIver, J
Meacher, D
Meadors, GD
Mehmet, M
Meidam, J
Meier, T
Melatos, A
Mendell, G
Mercer, RA
Meshkov, S
Messenger, C
Meyer, MS
Miao, H
Michel, C
Mikhailov, EE
Milano, L
Miller, J
Minenkov, Y
Mingarelli, CMF
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Moe, B
Mohan, M
Mohapatra, SRP
Mokler, F
Moraru, D
Moreno, G
Morgado, N
Mori, T
Morriss, SR
Mossavi, K
Mours, B
Mow-Lowry, CM
Mueller, CL
Mueller, G
Mukherjee, S
Mullavey, A
Munch, J
Murphy, D
Murray, PG
Mytidis, A
Nagy, MF
Kumar, DN
Nardecchia, I
Nash, T
Naticchioni, L
Nayak, R
Necula, V
Nelemans, G
Neri, I
Neri, M
Newton, G
Nguyen, T
Nishida, E
Nishizawa, A
Nitz, A
Nocera, F
Nolting, D
Normandin, ME
Nuttall, LK
Ochsner, E
O'Dell, J
Oelker, E
Ogin, GH
Oh, JJ
Oh, SH
Ohme, F
Oppermann, P
O'Reilly, B
Larcher, WO
O'Shaughnessy, R
Osthelder, C
Ottaway, DJ
Ottens, RS
Ou, J
Overmier, H
Owen, BJ
Padilla, C
Pai, A
Palomba, C
Pan, Y
Pankow, C
Paoletti, F
Paoletti, R
Papa, MA
Paris, H
Pasqualetti, A
Passaquieti, R
Passuello, D
Pedraza, M
Peiris, P
Penn, S
Perreca, A
Phelps, M
Pichot, M
Pickenpack, M
Piergiovanni, F
Pierro, V
Pinard, L
Pindor, B
Pinto, IM
Pitkin, M
Poeld, J
Poggiani, R
Poole, V
Poux, C
Predoi, V
Prestegard, T
Price, LR
Prijatelj, M
Principe, M
Privitera, S
Prix, R
Prodi, GA
Prokhorov, L
Puncken, O
Punturo, M
Puppo, P
Quetschke, V
Quintero, E
Quitzow-James, R
Raab, FJ
Rabeling, DS
Acz, IR'
Radkins, H
Raffai, P
Raja, S
Rajalakshmi, G
Rakhmanov, M
Ramet, C
Rapagnani, P
Raymond, V
Re, V
Reed, CM
Reed, T
Regimbau, T
Reid, S
Reitze, DH
Ricci, F
Riesen, R
Riles, K
Robertson, NA
Robinet, F
Rocchi, A
Roddy, S
Rodriguez, C
Rodruck, M
Roever, C
Rolland, L
Rollins, JG
Romano, JD
Romano, R
Romanov, G
Romie, JH
Rosinska, D
Rowan, S
Ruediger, A
Ruggi, P
Ryan, K
Salemi, F
Sammut, L
Sandberg, V
Sanders, J
Sannibale, V
Santiago-Prieto, I
Saracco, E
Sassolas, B
Sathyaprakash, BS
Saulson, PR
Savage, R
Schilling, R
Schnabel, R
Schofield, RMS
Schreiber, E
Schuette, D
Schulz, B
Schutz, BF
Schwinberg, P
Scott, J
Scott, SM
Seifert, F
Sellers, D
Sengupta, AS
Sentenac, D
Sergeev, A
Shaddock, D
Shah, S
Shahriar, MS
Shaltev, M
Shapiro, B
Shawhan, P
Shoemaker, DH
Sidery, TL
Siellez, K
Siemens, X
Sigg, D
Simakov, D
Singer, A
Singer, L
Sintes, AM
Skelton, GR
Slagmolen, BJJ
Slutsky, J
Smith, JR
Smith, MR
Smith, RJE
Smith-Lefebvre, ND
Soden, K
Son, EJ
Sorazu, B
Souradeep, T
Sperandio, L
Staley, A
Steinert, E
Steinlechner, J
Steinlechner, S
Steplewski, S
Stevens, D
Stochino, A
Stone, R
Strain, KA
Straniero, N
Strigin, S
Stroeer, AS
Sturani, R
Stuver, AL
Summerscales, TZ
Susmithan, S
Sutton, PJ
Swinkels, B
Szeifert, G
Tacca, M
Talukder, D
Tang, L
Tanner, DB
Tarabrin, SP
Taylor, R
Ter Braack, APM
Thirugnanasambandam, MP
Thomas, M
Thomas, P
Thorne, KA
Thorne, KS
Thrane, E
Tiwari, V
Tokmakov, KV
Tomlinson, C
Toncelli, A
Tonelli, M
Torre, O
Torres, CV
Torrie, CI
Travasso, F
Traylor, G
Tse, M
Ugolini, D
Unnikrishnan, CS
Vahlbruch, H
Vajente, G
Vallisneri, M
Van den Brand, JFJ
Van den Broeck, C
Van der Putten, S
Van der Sluys, MV
Van Heijningen, J
Van Veggel, AA
Vass, S
Vasuth, M
Vaulin, R
Vecchio, A
Vedovato, G
Veitch, J
Veitch, PJ
Venkateswara, K
Verkindt, D
Verma, S
Vetrano, F
Vicere, A
Vincent-Finley, R
Vinet, JY
Vitale, S
Vlcek, B
Vo, T
Vocca, H
Vorvick, C
Vousden, WD
Vrinceanu, D
Vyachanin, SP
Wade, A
Wade, L
Wade, M
Waldman, SJ
Walker, M
Wallace, L
Wan, Y
Wang, J
Wang, M
Wang, X
Wanner, A
Ward, RL
Was, M
Weaver, B
Wei, LW
Weinert, M
Weinstein, AJ
Weiss, R
Welborn, T
Wen, L
Wessels, P
West, M
Westphal, T
Wette, K
Whelan, JT
Whitcomb, SE
White, DJ
Whiting, BF
Wibowo, S
Wiesner, K
Wilkinson, C
Williams, L
Williams, R
Williams, T
Willis, JL
Willke, B
Wimmer, M
Winkelmann, L
Winkler, W
Wipf, CC
Wittel, H
Woan, G
Worden, J
Yablon, J
Yakushin, I
Yamamoto, H
Yancey, CC
Yang, H
Yeaton-Massey, D
Yoshida, S
Yum, H
Yvert, M
Zadrozny, A
Zanolin, M
Zendri, JP
Zhang, F
Zhang, L
Zhao, C
Zhu, H
Zhu, XJ
Zotov, N
Zucker, ME
Zweizig, J
Collaboration, LS
Collaboration, V
Buchner, S
Cognard, I
Corongiu, A
D'Amico, N
Espinoza, CM
Freire, PCC
Gotthelf, EV
Guillemot, L
Hessels, JWT
Hobbs, GB
Kramer, M
Lyne, AG
Marshall, FE
Possenti, A
Ransom, SM
Ray, PS
Roy, J
Stappers, BW
AF Aasi, J.
Abadie, J.
Abbott, B. P.
Abbott, R.
Abbott, T.
Abernathy, M. R.
Accadia, T.
Acernese, F.
Adams, C.
Adams, T.
Adhikari, R. X.
Affeldt, C.
Agathos, M.
Aggarwal, N.
Aguiar, O. D.
Ajith, P.
Allen, B.
Allocca, A.
Ceron, E. Amador
Amariutei, D.
Anderson, R. A.
Anderson, S. B.
Anderson, W. G.
Arai, K.
Araya, M. C.
Arceneaux, C.
Areeda, J.
Ast, S.
Aston, S. M.
Astone, P.
Aufmuth, P.
Aulbert, C.
Austin, L.
Aylott, B. E.
Babak, S.
Baker, P. T.
Ballardin, G.
Ballmer, S. W.
Barayoga, J. C.
Barker, D.
Barnum, S. H.
Barone, F.
Barr, B.
Barsotti, L.
Barsuglia, M.
Barton, M. A.
Bartos, I.
Bassiri, R.
Basti, A.
Batch, J.
Bauchrowitz, J.
Bauer, Th S.
Bebronne, M.
Behnke, B.
Bejger, M.
Beker, M. G.
Bell, A. S.
Bell, C.
Belopolski, I.
Bergmann, G.
Berliner, J. M.
Bersanetti, D.
Bertolini, A.
Bessis, D.
Betzwieser, J.
Beyersdorf, P. T.
Bhadbhade, T.
Bilenko, I. A.
Billingsley, G.
Birch, J.
Bitossi, M.
Bizouard, M. A.
Black, E.
Blackburn, J. K.
Blackburn, L.
Blair, D.
Blom, M.
Bock, O.
Bodiya, T. P.
Boer, M.
Bogan, C.
Bond, C.
Bondu, F.
Bonelli, L.
Bonnand, R.
Bork, R.
Born, M.
Boschi, V.
Bose, S.
Bosi, L.
Bowers, J.
Bradaschia, C.
Brady, P. R.
Braginsky, V. B.
Branchesi, M.
Brannen, C. A.
Brau, J. E.
Breyer, J.
Briant, T.
Bridges, D. O.
Brillet, A.
Brinkmann, M.
Brisson, V.
Britzger, M.
Brooks, A. F.
Brown, D. A.
Brown, D. D.
Brueckner, F.
Bulik, T.
Bulten, H. J.
Buonanno, A.
Buskulic, D.
Buy, C.
Byer, R. L.
Cadonati, L.
Cagnoli, G.
Bustillo, J. Calderon
Calloni, E.
Camp, J. B.
Campsie, P.
Cannon, K. C.
Canuel, B.
Cao, J.
Capano, C. D.
Carbognani, F.
Carbone, L.
Caride, S.
Castiglia, A.
Caudill, S.
Cavaglia, M.
Cavalier, F.
Cavalieri, R.
Cella, G.
Cepeda, C.
Cesarini, E.
Chakraborty, R.
Chalermsongsak, T.
Chao, S.
Charlton, P.
Chassande-Mottin, E.
Chen, X.
Chen, Y.
Chincarini, A.
Chiummo, A.
Cho, H. S.
Chow, J.
Christensen, N.
Chu, Q.
Chua, S. S. Y.
Chung, S.
Ciani, G.
Clara, F.
Clark, D. E.
Clark, J. A.
Cleva, F.
Coccia, E.
Cohadon, P-F.
Colla, A.
Colombini, M.
Jr, M. Constancio
Conte, A.
Conte, R.
Cook, D.
Corbitt, T. R.
Cordier, M.
Cornish, N.
Corsi, A.
Costa, C. A.
Coughlin, M. W.
Coulon, J-P.
Countryman, S.
Couvares, P.
Coward, D. M.
Cowart, M.
Coyne, D. C.
Craig, K.
Creighton, J. D. E.
Creighton, T. D.
Crowder, S. G.
Cumming, A.
Cunningham, L.
Cuoco, E.
Dahl, K.
Dal Canton, T.
Damjanic, M.
Danilishin, S. L.
D'Antonio, S.
Danzmann, K.
Dattilo, V.
Daudert, B.
Daveloza, H.
Davier, M.
Davies, G. S.
Daw, E. J.
Day, R.
Dayanga, T.
De Rosa, R.
Debreczeni, G.
Degallaix, J.
Del Pozzo, W.
Deleeuw, E.
Deleglise, S.
Denker, T.
Dent, T.
Dereli, H.
Dergachev, V.
DeRosa, R.
DeSalvo, R.
Dhurandhar, S.
Di Fiore, L.
Di Lieto, A.
Di Palma, I.
Di Virgilio, A.
Diaz, M.
Dietz, A.
Dmitry, K.
Donovan, F.
Dooley, K. L.
Doravari, S.
Drago, M.
Drever, R. W. P.
Driggers, J. C.
Du, Z.
Dumas, J-C.
Dwyer, S.
Eberle, T.
Edwards, M.
Effler, A.
Ehrens, P.
Eichholz, J.
Eikenberry, S. S.
Endroczi, G.
Essick, R.
Etzel, T.
Evans, K.
Evans, M.
Evans, T.
Factourovich, M.
Fafone, V.
Fairhurst, S.
Fang, Q.
Farinon, S.
Farr, B.
Farr, W.
Favata, M.
Fazi, D.
Fehrmann, H.
Feldbaum, D.
Ferrante, I.
Ferrini, F.
Fidecaro, F.
Finn, L. S.
Fiori, I.
Fisher, R.
Flaminio, R.
Foley, E.
Foley, S.
Forsi, E.
Fotopoulos, N.
Fournier, J-D.
Franco, S.
Frasca, S.
Frasconi, F.
Frede, M.
Frei, M.
Frei, Z.
Freise, A.
Frey, R.
Fricke, T. T.
Fritschel, P.
Frolov, V. V.
Fujimoto, M-K.
Fulda, P.
Fyffe, M.
Gair, J.
Gammaitoni, L.
Garcia, J.
Garufi, F.
Gehrels, N.
Gemme, G.
Genin, E.
Gennai, A.
Gergely, L.
Ghosh, S.
Giaime, J. A.
Giampanis, S.
Giardina, K. D.
Giazotto, A.
Gil-Casanova, S.
Gill, C.
Gleason, J.
Goetz, E.
Goetz, R.
Gondan, L.
Gonzalez, G.
Gordon, N.
Gorodetsky, M. L.
Gossan, S.
Gossler, S.
Gouaty, R.
Graef, C.
Graff, P. B.
Granata, M.
Grant, A.
Gras, S.
Gray, C.
Greenhalgh, R. J. S.
Gretarsson, A. M.
Griffo, C.
Groot, P.
Grote, H.
Grover, K.
Grunewald, S.
Guidi, G. M.
Guido, C.
Gushwa, K. E.
Gustafson, E. K.
Gustafson, R.
Hall, B.
Hall, E.
Hammer, D.
Hammond, G.
Hanke, M.
Hanks, J.
Hanna, C.
Hanson, J.
Harms, J.
Harry, G. M.
Harry, I. W.
Harstad, E. D.
Hartman, M. T.
Haughian, K.
Hayama, K.
Heefner, J.
Heidmann, A.
Heintze, M.
Heitmann, H.
Hello, P.
Hemming, G.
Hendry, M.
Heng, I. S.
Heptonstall, A. W.
Heurs, M.
Hild, S.
Hoak, D.
Hodge, K. A.
Holt, K.
Holtrop, M.
Hong, T.
Hooper, S.
Horrom, T.
Hosken, D. J.
Hough, J.
Howell, E. J.
Hu, Y.
Hua, Z.
Huang, V.
Huerta, E. A.
Hughey, B.
Husa, S.
Huttner, S. H.
Huynh, M.
Huynh-Dinh, T.
Iafrate, J.
Ingram, D. R.
Inta, R.
Isogai, T.
Ivanov, A.
Iyer, B. R.
Izumi, K.
Jacobson, M.
James, E.
Jang, H.
Jang, Y. J.
Jaranowski, P.
Jimenez-Forteza, F.
Johnson, W. W.
Jones, D.
Jones, D. I.
Jones, R.
Jonker, R. J. G.
Ju, L.
Haris, K.
Kalmus, P.
Kalogera, V.
Kandhasamy, S.
Kang, G.
Kanner, J. B.
Kasprzack, M.
Kasturi, R.
Katsavounidis, E.
Katzman, W.
Kaufer, H.
Kaufman, K.
Kawabe, K.
Kawamura, S.
Kawazoe, F.
Kefelian, F.
Keitel, D.
Kelley, D. B.
Kells, W.
Keppel, D. G.
Khalaidovski, A.
Khalili, F. Y.
Khazanov, E. A.
Kim, B. K.
Kim, C.
Kim, K.
Kim, N.
Kim, W.
Kim, Y. -M.
King, E. J.
King, P. J.
Kinzel, D. L.
Kissel, J. S.
Klimenko, S.
Kline, J.
Koehlenbeck, S.
Kokeyama, K.
Kondrashov, V.
Koranda, S.
Korth, W. Z.
Kowalska, I.
Kozak, D.
Kremin, A.
Kringel, V.
Krishnan, B.
Krolak, A.
Kucharczyk, C.
Kudla, S.
Kuehn, G.
Kumar, A.
Kumar, P.
Kumar, R.
Kurdyumov, R.
Kwee, P.
Landry, M.
Lantz, B.
Larson, S.
Lasky, P. D.
Lawrie, C.
Lazzarini, A.
Le Roux, A.
Leaci, P.
Lebigot, E. O.
Lee, C. -H.
Lee, H. K.
Lee, H. M.
Lee, J.
Lee, J.
Leonardi, M.
Leong, J. R.
Leroy, N.
Letendre, N.
Levine, B.
Lewis, J. B.
Lhuillier, V.
Li, T. G. F.
Lin, A. C.
Littenberg, T. B.
Litvine, V.
Liu, F.
Liu, H.
Liu, Y.
Liu, Z.
Lloyd, D.
Lockerbie, N. A.
Lockett, V.
Lodhia, D.
Loew, K.
Logue, J.
Lombardi, A. L.
Lorenzini, M.
Loriette, V.
Lormand, M.
Losurdo, G.
Lough, J.
Luan, J.
Lubinski, M. J.
Lueck, H.
Lundgren, A. P.
Macarthur, J.
Macdonald, E.
Machenschalk, B.
MacInnis, M.
Macleod, D. M.
Magana-Sandoval, F.
Mageswaran, M.
Mailand, K.
Majorana, E.
Maksimovic, I.
Malvezzi, V.
Man, N.
Manca, G. M.
Mandel, I.
Mandic, V.
Mangano, V.
Mantovani, M.
Marchesoni, F.
Marion, F.
Marka, S.
Marka, Z.
Markosyan, A.
Maros, E.
Marque, J.
Martelli, F.
Martin, I. W.
Martin, R. M.
Martinelli, L.
Martynov, D.
Marx, J. N.
Mason, K.
Masserot, A.
Massinger, T. J.
Matichard, F.
Matone, L.
Matzner, R. A.
Mavalvala, N.
May, G.
Mazumder, N.
Mazzolo, G.
McCarthy, R.
McClelland, D. E.
McGuire, S. C.
McIntyre, G.
McIver, J.
Meacher, D.
Meadors, G. D.
Mehmet, M.
Meidam, J.
Meier, T.
Melatos, A.
Mendell, G.
Mercer, R. A.
Meshkov, S.
Messenger, C.
Meyer, M. S.
Miao, H.
Michel, C.
Mikhailov, E. E.
Milano, L.
Miller, J.
Minenkov, Y.
Mingarelli, C. M. F.
Mitra, S.
Mitrofanov, V. P.
Mitselmakher, G.
Mittleman, R.
Moe, B.
Mohan, M.
Mohapatra, S. R. P.
Mokler, F.
Moraru, D.
Moreno, G.
Morgado, N.
Mori, T.
Morriss, S. R.
Mossavi, K.
Mours, B.
Mow-Lowry, C. M.
Mueller, C. L.
Mueller, G.
Mukherjee, S.
Mullavey, A.
Munch, J.
Murphy, D.
Murray, P. G.
Mytidis, A.
Nagy, M. F.
Kumar, D. Nanda
Nardecchia, I.
Nash, T.
Naticchioni, L.
Nayak, R.
Necula, V.
Nelemans, G.
Neri, I.
Neri, M.
Newton, G.
Nguyen, T.
Nishida, E.
Nishizawa, A.
Nitz, A.
Nocera, F.
Nolting, D.
Normandin, M. E.
Nuttall, L. K.
Ochsner, E.
O'Dell, J.
Oelker, E.
Ogin, G. H.
Oh, J. J.
Oh, S. H.
Ohme, F.
Oppermann, P.
O'Reilly, B.
Larcher, W. Ortega
O'Shaughnessy, R.
Osthelder, C.
Ottaway, D. J.
Ottens, R. S.
Ou, J.
Overmier, H.
Owen, B. J.
Padilla, C.
Pai, A.
Palomba, C.
Pan, Y.
Pankow, C.
Paoletti, F.
Paoletti, R.
Papa, M. A.
Paris, H.
Pasqualetti, A.
Passaquieti, R.
Passuello, D.
Pedraza, M.
Peiris, P.
Penn, S.
Perreca, A.
Phelps, M.
Pichot, M.
Pickenpack, M.
Piergiovanni, F.
Pierro, V.
Pinard, L.
Pindor, B.
Pinto, I. M.
Pitkin, M.
Poeld, J.
Poggiani, R.
Poole, V.
Poux, C.
Predoi, V.
Prestegard, T.
Price, L. R.
Prijatelj, M.
Principe, M.
Privitera, S.
Prix, R.
Prodi, G. A.
Prokhorov, L.
Puncken, O.
Punturo, M.
Puppo, P.
Quetschke, V.
Quintero, E.
Quitzow-James, R.
Raab, F. J.
Rabeling, D. S.
Acz, I. R. '
Radkins, H.
Raffai, P.
Raja, S.
Rajalakshmi, G.
Rakhmanov, M.
Ramet, C.
Rapagnani, P.
Raymond, V.
Re, V.
Reed, C. M.
Reed, T.
Regimbau, T.
Reid, S.
Reitze, D. H.
Ricci, F.
Riesen, R.
Riles, K.
Robertson, N. A.
Robinet, F.
Rocchi, A.
Roddy, S.
Rodriguez, C.
Rodruck, M.
Roever, C.
Rolland, L.
Rollins, J. G.
Romano, J. D.
Romano, R.
Romanov, G.
Romie, J. H.
Rosinska, D.
Rowan, S.
Ruediger, A.
Ruggi, P.
Ryan, K.
Salemi, F.
Sammut, L.
Sandberg, V.
Sanders, J.
Sannibale, V.
Santiago-Prieto, I.
Saracco, E.
Sassolas, B.
Sathyaprakash, B. S.
Saulson, P. R.
Savage, R.
Schilling, R.
Schnabel, R.
Schofield, R. M. S.
Schreiber, E.
Schuette, D.
Schulz, B.
Schutz, B. F.
Schwinberg, P.
Scott, J.
Scott, S. M.
Seifert, F.
Sellers, D.
Sengupta, A. S.
Sentenac, D.
Sergeev, A.
Shaddock, D.
Shah, S.
Shahriar, M. S.
Shaltev, M.
Shapiro, B.
Shawhan, P.
Shoemaker, D. H.
Sidery, T. L.
Siellez, K.
Siemens, X.
Sigg, D.
Simakov, D.
Singer, A.
Singer, L.
Sintes, A. M.
Skelton, G. R.
Slagmolen, B. J. J.
Slutsky, J.
Smith, J. R.
Smith, M. R.
Smith, R. J. E.
Smith-Lefebvre, N. D.
Soden, K.
Son, E. J.
Sorazu, B.
Souradeep, T.
Sperandio, L.
Staley, A.
Steinert, E.
Steinlechner, J.
Steinlechner, S.
Steplewski, S.
Stevens, D.
Stochino, A.
Stone, R.
Strain, K. A.
Straniero, N.
Strigin, S.
Stroeer, A. S.
Sturani, R.
Stuver, A. L.
Summerscales, T. Z.
Susmithan, S.
Sutton, P. J.
Swinkels, B.
Szeifert, G.
Tacca, M.
Talukder, D.
Tang, L.
Tanner, D. B.
Tarabrin, S. P.
Taylor, R.
Ter Braack, A. P. M.
Thirugnanasambandam, M. P.
Thomas, M.
Thomas, P.
Thorne, K. A.
Thorne, K. S.
Thrane, E.
Tiwari, V.
Tokmakov, K. V.
Tomlinson, C.
Toncelli, A.
Tonelli, M.
Torre, O.
Torres, C. V.
Torrie, C. I.
Travasso, F.
Traylor, G.
Tse, M.
Ugolini, D.
Unnikrishnan, C. S.
Vahlbruch, H.
Vajente, G.
Vallisneri, M.
Van den Brand, J. F. J.
Van den Broeck, C.
Van der Putten, S.
Van der Sluys, M. V.
Van Heijningen, J.
Van Veggel, A. A.
Vass, S.
Vasuth, M.
Vaulin, R.
Vecchio, A.
Vedovato, G.
Veitch, J.
Veitch, P. J.
Venkateswara, K.
Verkindt, D.
Verma, S.
Vetrano, F.
Vicere, A.
Vincent-Finley, R.
Vinet, J. -Y.
Vitale, S.
Vlcek, B.
Vo, T.
Vocca, H.
Vorvick, C.
Vousden, W. D.
Vrinceanu, D.
Vyachanin, S. P.
Wade, A.
Wade, L.
Wade, M.
Waldman, S. J.
Walker, M.
Wallace, L.
Wan, Y.
Wang, J.
Wang, M.
Wang, X.
Wanner, A.
Ward, R. L.
Was, M.
Weaver, B.
Wei, L. -W.
Weinert, M.
Weinstein, A. J.
Weiss, R.
Welborn, T.
Wen, L.
Wessels, P.
West, M.
Westphal, T.
Wette, K.
Whelan, J. T.
Whitcomb, S. E.
White, D. J.
Whiting, B. F.
Wibowo, S.
Wiesner, K.
Wilkinson, C.
Williams, L.
Williams, R.
Williams, T.
Willis, J. L.
Willke, B.
Wimmer, M.
Winkelmann, L.
Winkler, W.
Wipf, C. C.
Wittel, H.
Woan, G.
Worden, J.
Yablon, J.
Yakushin, I.
Yamamoto, H.
Yancey, C. C.
Yang, H.
Yeaton-Massey, D.
Yoshida, S.
Yum, H.
Yvert, M.
Zadrozny, A.
Zanolin, M.
Zendri, J. -P.
Zhang, F.
Zhang, L.
Zhao, C.
Zhu, H.
Zhu, X. J.
Zotov, N.
Zucker, M. E.
Zweizig, J.
Collaboration, Ligo Sci
Collaboration, Virgo
Buchner, S.
Cognard, I.
Corongiu, A.
D'Amico, N.
Espinoza, C. M.
Freire, P. C. C.
Gotthelf, E. V.
Guillemot, L.
Hessels, J. W. T.
Hobbs, G. B.
Kramer, M.
Lyne, A. G.
Marshall, F. E.
Possenti, A.
Ransom, S. M.
Ray, P. S.
Roy, J.
Stappers, B. W.
TI GRAVITATIONAL WAVES FROM KNOWN PULSARS: RESULTS FROM THE INITIAL
DETECTOR ERA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational waves; pulsars: general
ID GAMMA-RAY PULSARS; SPIN-DOWN LIMIT; NEUTRON-STARS; CRAB PULSAR;
GLOBULAR-CLUSTERS; PSR J1734-3333; PROPER MOTION; WIND TORI; EMISSION;
DISCOVERY
AB We present the results of searches for gravitational waves from a large selection of pulsars using data from the most recent science runs (S6, VSR2 and VSR4) of the initial generation of interferometric gravitational wave detectors LIGO (Laser Interferometric Gravitational-wave Observatory) and Virgo. We do not see evidence for gravitational wave emission from any of the targeted sources but produce upper limits on the emission amplitude. We highlight the results from seven young pulsars with large spin-down luminosities. We reach within a factor of five of the canonical spin-down limit for all seven of these, whilst for the Crab and Vela pulsars we further surpass their spin-down limits. We present new or updated limits for 172 other pulsars (including both young and millisecond pulsars). Now that the detectors are undergoing major upgrades, and, for completeness, we bring together all of the most up-to-date results from all pulsars searched for during the operations of the first-generation LIGO, Virgo and GEO600 detectors. This gives a total of 195 pulsars including the most recent results described in this paper.
C1 [Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Ajith, P.; Anderson, R. A.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Barayoga, J. C.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chakraborty, R.; Chalermsongsak, T.; Coyne, D. C.; Daudert, B.; Dergachev, V.; Driggers, J. C.; Etzel, T.; Fotopoulos, N.; Gushwa, K. E.; Gustafson, E. K.; Hall, E.; Harms, J.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D.; Lazzarini, A.; Lewis, J. B.; Litvine, V.; Lloyd, D.; Mageswaran, M.; Mailand, K.; Maros, E.; Martynov, D.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Nash, T.; Ogin, G. H.; Osthelder, C.; Pedraza, M.; Phelps, M.; Poux, C.; Price, L. R.; Privitera, S.; Quintero, E.; Raymond, V.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Seifert, F.; Singer, A.; Singer, L.; Smith, M. R.; Smith-Lefebvre, N. D.; Taylor, R.; Thirugnanasambandam, M. P.; Thrane, E.; Torrie, C. I.; Vass, S.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Williams, R.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Abbott, T.; Bowers, J.; Corbitt, T. R.; DeRosa, R.; Effler, A.; Giaime, J. A.; Gonzalez, G.; Iafrate, J.; Johnson, W. W.; Kokeyama, K.; Kudla, S.; May, G.; Mullavey, A.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Accadia, T.; Bebronne, M.; Buskulic, D.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Verkindt, D.; Yvert, M.] Univ Savoie, CNRS IN2P3, LAPP, F-74941 Annecy Le Vieux, France.
[Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Garufi, F.; Milano, L.; Romano, R.] Ist Nazl Fis Nucl, Sez Napoli, 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.; Doravari, S.; Evans, T.; Feldbaum, D.; Forsi, E.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Guido, C.; Hanson, J.; Heintze, M.; 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.; Thomas, M.; Thorne, K. A.; Traylor, G.; Welborn, T.; Yakushin, I.] Livingston Observ, LIGO, Livingston, LA 70754 USA.
[Adams, T.; Edwards, M.; Fairhurst, S.; Liu, H.; Macdonald, E.; Macleod, D. M.; Nuttall, L. K.; Ohme, F.; Predoi, V.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Affeldt, C.; Allen, B.; Aulbert, C.; Bauchrowitz, J.; Bergmann, G.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Dal Canton, T.; Damjanic, M.; Danzmann, K.; Denker, T.; Dent, T.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Hanke, M.; Heurs, M.; Kawazoe, F.; Keitel, D.; Keppel, D. G.; Khalaidovski, A.; Koehlenbeck, S.; Kringel, V.; Krishnan, B.; Kuehn, G.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Manca, G. M.; Mazzolo, G.; Mehmet, M.; Mokler, F.; Mossavi, K.; Mow-Lowry, C. M.; Oppermann, P.; Pickenpack, M.; Poeld, J.; Prijatelj, M.; Prix, R.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schreiber, E.; Schuette, D.; Schulz, B.; Shaltev, M.; Simakov, D.; Slutsky, J.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Wanner, A.; Was, M.; 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.
[Agathos, M.; Bauer, Th S.; Beker, M. G.; Bertolini, A.; Blom, M.; Bulten, H. J.; Del Pozzo, W.; Jonker, R. J. G.; Li, T. G. F.; Meidam, J.; Nelemans, G.; Rabeling, D. S.; Shah, S.; Ter Braack, A. P. M.; Van den Brand, J. F. J.; Van den Broeck, C.; Van der Putten, S.; Van der Sluys, M. V.; Van Heijningen, J.; Veitch, J.; Vitale, S.] Nikhef, NL-1098 XG Amsterdam, Netherlands.
[Aggarwal, N.; Barnum, S. H.; Barsotti, L.; Bodiya, T. P.; Donovan, F.; Essick, R.; Evans, M.; Foley, S.; Fritschel, P.; Gras, S.; Isogai, T.; Katsavounidis, E.; Kissel, J. S.; Kwee, P.; Lee, J.; MacInnis, M.; Mason, K.; Matichard, F.; Mavalvala, N.; Mittleman, R.; Oelker, E.; Shoemaker, D. H.; Vaulin, R.; Vitale, S.; Waldman, S. J.; Weiss, R.; Wipf, C. C.; Zhang, F.; Zucker, M. E.] MIT, LIGO, Cambridge, MA 02139 USA.
[Aguiar, O. D.; Jr, M. Constancio; Costa, C. A.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Allen, B.; Ceron, E. Amador; Anderson, W. G.; Brady, P. R.; Caudill, S.; Creighton, J. D. E.; Giampanis, S.; Hammer, D.; Huynh, M.; Kline, J.; Koranda, S.; Mercer, R. A.; Moe, B.; Ochsner, E.; O'Shaughnessy, R.; Pankow, C.; Papa, M. A.; Siemens, X.; Skelton, G. R.; Soden, K.; Vlcek, B.; Wade, L.; Wade, M.; Wibowo, S.; Williams, T.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Allen, B.; Ast, S.; Aufmuth, P.; Danzmann, K.; Kaufer, H.; Lueck, H.; Meier, T.; Schnabel, R.; Vahlbruch, H.; Willke, B.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Allocca, A.; Basti, A.; Bitossi, M.; Bonelli, L.; Boschi, V.; Bradaschia, C.; Cella, G.; 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.
[Allocca, A.; Paoletti, R.; Torre, O.] Univ Siena, I-53100 Siena, Italy.
[Amariutei, D.; Ciani, G.; Deleeuw, E.; Ehrens, P.; Eichholz, J.; Eikenberry, S. S.; Feldbaum, D.; Fulda, P.; Gleason, J.; Goetz, R.; Hartman, M. T.; Heintze, M.; Klimenko, S.; Liu, Z.; Martin, R. M.; Mitselmakher, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Kumar, D. Nanda; Necula, V.; Ottens, R. S.; Reitze, D. H.; Tanner, D. B.; Tiwari, V.; Whiting, B. F.; Williams, L.] Univ Florida, Gainesville, FL 32611 USA.
[Arceneaux, C.; Cavaglia, M.; Dietz, A.] Univ Mississippi, University, MS 38677 USA.
[Areeda, J.; Foley, E.; Griffo, C.; Lee, J.; Lockett, V.; Magana-Sandoval, F.; Padilla, C.; Smith, J. R.] Calif State Univ Fullerton, Fullerton, CA 92831 USA.
[Astone, P.; Colla, A.; Conte, A.; Frasca, S.; Majorana, E.; Mangano, V.; Nardecchia, I.; Naticchioni, L.; Palomba, C.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
[Aylott, B. E.; Bond, C.; Brown, D. D.; Brueckner, F.; Carbone, L.; Freise, A.; Grover, K.; Lodhia, D.; Mandel, I.; Mingarelli, C. M. F.; Sidery, T. L.; Smith, R. J. E.; Vecchio, A.; Vousden, W. D.; Wang, M.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Babak, S.; Behnke, B.; Grunewald, S.; Leaci, P.; Papa, M. A.; Schutz, B. F.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Baker, P. T.; Cornish, N.] Montana State Univ, Bozeman, MT 59717 USA.
[Ballardin, G.; Canuel, B.; Carbognani, F.; Cavalieri, R.; Chiummo, A.; Cuoco, E.; Dattilo, V.; Day, R.; 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.] EGO, I-56021 Pisa, Italy.
[Ballmer, S. W.; Brown, D. A.; Couvares, P.; Fisher, R.; Harry, I. W.; Huerta, E. A.; Kelley, D. B.; Kumar, P.; Lough, J.; Massinger, T. J.; Mohapatra, S. R. P.; Nitz, A.; Perreca, A.; Saulson, P. R.; West, M.] Syracuse Univ, Syracuse, NY 13244 USA.
[Barker, D.; Barton, M. A.; Batch, J.; Berliner, J. M.; Clara, F.; Cook, D.; Dwyer, S.; Garcia, J.; Gray, C.; Hanks, J.; Ingram, D. R.; Izumi, K.; Jones, D.; Kawabe, K.; Landry, M.; Levine, B.; Lhuillier, V.; Lubinski, M. J.; McCarthy, R.; Mendell, G.; Moraru, D.; Moreno, G.; Paris, H.; Raab, F. J.; Radkins, H.; Reed, C. M.; Rodruck, M.; Ryan, K.; Sandberg, V.; Savage, R.; Schwinberg, P.; Sigg, D.; Steinert, E.; Thomas, P.; Vo, T.; Vorvick, C.; Weaver, B.; Wilkinson, C.; Worden, J.] Hanford Observ, LIGO, Richland, WA 99352 USA.
[Barr, B.; Bassiri, R.; Bell, A. S.; Bell, C.; Campsie, P.; Craig, K.; Cumming, A.; Cunningham, L.; Davies, G. S.; Evans, K.; Gill, C.; Gordon, N.; Grant, A.; Hammond, G.; Haughian, K.; Hendry, M.; Heng, I. S.; Hild, S.; Hough, J.; Hu, Y.; Huttner, S. H.; Jones, R.; Kumar, R.; Lawrie, C.; Logue, J.; Macarthur, J.; Martin, I. W.; Messenger, C.; Murray, P. G.; Newton, G.; Pitkin, M.; Robertson, N. A.; Rowan, S.; Santiago-Prieto, I.; Scott, J.; Sorazu, B.; Strain, K. A.; Torrie, C. I.; Van Veggel, A. A.; Woan, G.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Buy, C.; Chassande-Mottin, E.; Tacca, M.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, Observ Paris, F-75205 Paris 13, France.
[Bartos, I.; Belopolski, I.; Countryman, S.; Factourovich, M.; Marka, S.; Marka, Z.; Matone, L.; Murphy, D.; Raffai, P.; Staley, A.; Tse, M.; Gotthelf, E. V.] Columbia Univ, New York, NY 10027 USA.
[Bassiri, R.; Bhadbhade, T.; Byer, R. L.; Clark, D. E.; Kim, N.; Kucharczyk, C.; Kurdyumov, R.; Lantz, B.; Lin, A. C.; Markosyan, A.; Shapiro, B.] Stanford Univ, Stanford, CA 94305 USA.
[Basti, A.; Bonelli, L.; Di Lieto, A.; Ferrante, I.; Fidecaro, F.; Passaquieti, R.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Vajente, G.] Univ Pisa, I-56127 Pisa, Italy.
[Bejger, M.; Rosinska, D.] Polish Acad Sci, CAMK, PL-00716 Warsaw, Poland.
[Bersanetti, D.; Chincarini, A.; Farinon, S.; Gemme, G.; Neri, M.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy.
[Bersanetti, D.; Neri, M.] Univ Genoa, I-16146 Genoa, Italy.
[Bessis, D.; Creighton, T. D.; Daveloza, H.; Diaz, M.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E.; Larcher, W. Ortega; Puncken, O.; Quetschke, V.; Rakhmanov, M.; Romano, J. D.; Stone, R.; Stroeer, A. S.; Tang, L.; Torres, C. V.; Vrinceanu, D.] 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.; Dmitry, K.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L.; Strigin, S.; Vyachanin, 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.; Marshall, F. E.] Univ Paris 11, CNRS IN2P3, LAL, F-91898 Orsay, France.
[Blackburn, L.; Camp, J. B.; Gehrels, N.; Graff, P. B.; Kanner, J. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blair, D.; Chen, X.; Chu, Q.; Chung, S.; Coward, D. M.; Danilishin, S. L.; Dumas, J-C.; Fang, Q.; Hooper, S.; Howell, E. J.; Ju, L.; Susmithan, S.; Verma, S.; Wen, L.; Whitcomb, S. E.; Zhao, C.; Zhu, X. J.] Univ Western Australia, Crawley, WA 6009, Australia.
[Boer, M.; Brillet, A.; Cleva, F.; Coulon, J-P.; Dereli, H.; Fournier, J-D.; Heitmann, H.; Kefelian, F.; Man, N.; Martinelli, L.; Meacher, D.; Pichot, M.; Regimbau, T.; Siellez, K.; Vinet, J. -Y.; Wei, L. -W.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice, France.
[Bondu, F.] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France.
[Bonnand, R.; Cagnoli, G.; Degallaix, J.; Flaminio, R.; Granata, M.; Michel, C.; Morgado, N.; Pinard, L.; Saracco, E.; Sassolas, B.; Straniero, N.] Univ Lyon, CNRS IN2P3, LMA, F-69622 Lyon, France.
[Bose, S.; Brannen, C. A.; Dayanga, T.; Ghosh, S.; Hall, B.; Poole, V.; Steplewski, S.] Washington State Univ, Pullman, WA 99164 USA.
[Bosi, L.; Colombini, M.; Gammaitoni, L.; Marchesoni, F.; Neri, I.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Branchesi, M.; Guidi, G. M.; Losurdo, G.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Florence, Italy.
[Branchesi, M.; Guidi, G. M.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Univ Urbino Carlo Bo, I-61029 Urbino, Italy.
[Brau, J. E.; Frey, R.; Harstad, E. D.; Quitzow-James, R.; Schofield, R. M. S.; Talukder, D.] Univ Oregon, Eugene, OR 97403 USA.
[Briant, T.; Cohadon, P-F.; Deleglise, S.; Heidmann, A.] Univ Paris 06, CNRS, ENS, Lab Kastler Brossel, F-75005 Paris, France.
[Bulik, T.; Kowalska, I.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
[Bulten, H. J.; Rabeling, D. S.; Van den Brand, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands.
[Buonanno, A.; Capano, C. D.; Pan, Y.; Shawhan, P.; Yancey, C. C.] Univ Maryland, College Pk, MD 20742 USA.
[Cadonati, L.; Clark, J. A.; Hoak, D.; Lombardi, A. L.; McIver, J.] Univ Massachusetts, Amherst, MA 01003 USA.
[Bustillo, J. Calderon; Gil-Casanova, S.; Husa, S.; Jimenez-Forteza, F.; Sintes, A. M.] Univ Illes Balears, E-07122 Palma De Mallorca, Spain.
[Calloni, E.; De Rosa, R.; Garufi, F.; Milano, L.] Univ Naples Federico II, I-80126 Naples, Italy.
[Cannon, K. C.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Cao, J.; Du, Z.; Hua, Z.; Lebigot, E. O.; Liu, Y.; Wan, Y.; Wang, X.] Tsinghua Univ, Beijing 100084, Peoples R China.
[Caride, S.; Gustafson, R.; Meadors, G. D.; Riles, K.; Sanders, J.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Castiglia, A.; Frei, M.; Mohapatra, S. R. P.; Peiris, P.; Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Cesarini, E.; D'Antonio, S.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Minenkov, Y.; Re, V.; Rocchi, A.; Sperandio, L.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Chao, S.; Huang, V.; Ou, J.; Wang, J.] Natl Tsing Hua Univ, Hsinchu 300, Taiwan.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Chen, Y.; Gossan, S.; Hong, T.; Kaufman, K.; Luan, J.; Miao, H.; Thorne, K. S.; Vallisneri, M.; Yang, H.] CALTECH, CaRT, Pasadena, CA 91125 USA.
[Cho, H. S.; Kim, Y. -M.; Lee, C. -H.] Pusan Natl Univ, Pusan 609735, South Korea.
[Chow, J.; Chua, S. S. Y.; Inta, R.; McClelland, D. E.; Miller, J.; Nguyen, T.; Scott, S. M.; Shaddock, D.; Slagmolen, B. J. J.; Stochino, A.; Wade, A.; Ward, R. L.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Christensen, N.] Carleton Coll, Northfield, MN 55057 USA.
[Coccia, E.] Gran Sasso Sci Inst, Ist Nazl Fis Nucl, I-67100 Laquila, Italy.
[Coccia, E.; Fafone, V.; Re, V.; Sperandio, L.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Colla, A.; Conte, A.; Frasca, S.; Mangano, V.; Nardecchia, I.; Naticchioni, L.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Conte, R.; DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[Conte, R.; DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Ist Nazl Fis Nucl, Sez Napoli, Milan, Italy.
[Corsi, A.] George Washington Univ, Washington, DC 20052 USA.
[Coughlin, M. W.; Gair, J.] Univ Cambridge, Cambridge CB2 1TN, England.
[Crowder, S. G.; Kandhasamy, S.; Kremin, A.; Mandic, V.; Prestegard, T.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Daw, E. J.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[Debreczeni, G.; Endroczi, G.; Nagy, M. F.; Acz, I. R. '; Vasuth, M.] RMKI, Wigner RCP, H-1121 Budapest, Hungary.
[Dhurandhar, S.; Mitra, S.; Souradeep, T.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Drago, M.; Leonardi, M.; Prodi, G. A.] Ist Nazl Fis Nucl, Grp Collegato Trento, I-38050 Povo, Trento, Italy.
[Drago, M.; Leonardi, M.; Prodi, G. A.] Univ Trento, I-38050 Povo, Trento, Italy.
[Drever, R. W. P.] CALTECH, Pasadena, CA 91125 USA.
[Farr, B.; Farr, W.; Fazi, D.; Jang, Y. J.; Kalogera, V.; Littenberg, T. B.; Rodriguez, C.; Shahriar, M. S.; Stevens, D.; Yablon, J.; Yum, H.] Northwestern Univ, Evanston, IL 60208 USA.
[Favata, M.] Montclair State Univ, Montclair, NJ 07043 USA.
[Owen, B. J.; Zhu, H.] Penn State Univ, University Pk, PA 16802 USA.
[Frei, Z.; Gergely, L.; Gondan, L.; Raffai, P.; Szeifert, G.] Eotvos Lorand Univ, MTA, H-1117 Budapest, Hungary.
[Fujimoto, M-K.; Hayama, K.; Kawamura, S.; Mori, T.; Nishida, E.; Nishizawa, A.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Gammaitoni, L.; Neri, I.; Travasso, F.; Vocca, H.] Univ Perugia, I-06123 Perugia, Italy.
[Greenhalgh, R. J. S.; O'Dell, J.] HSIC, Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Gretarsson, A. M.; Hughey, B.; Loew, K.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Groot, P.; Nelemans, G.; Shah, S.; Van der Sluys, M. V.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Hanna, C.] Perimeter Inst Theoret Phys, Toronto, ON N2L 2Y5, Canada.
[Harry, G. M.] Amer Univ, Washington, DC 20016 USA.
[Holtrop, M.] Univ New Hampshire, Durham, NH 03824 USA.
[Horrom, T.; Mikhailov, E. E.; Romanov, G.] Coll William & Mary, Williamsburg, VA 23187 USA.
[Hosken, D. J.; Kim, W.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Iyer, B. R.] Raman Res Inst, Bangalore 560080, Karnataka, India.
[Jang, H.; Kang, G.; Kim, B. K.; Kim, C.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea.
[Jaranowski, P.] Bialystok Univ, PL-15424 Bialystok, Poland.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Haris, K.; Mazumder, N.; Pai, A.] IISER TVM, Trivandrum 695016, Kerala, India.
[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.; Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Krolak, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Kumar, A.] Inst Plasma Res, Bhat 382428, Gandhinagar, India.
[Larson, S.] Utah State Univ, Logan, UT 84322 USA.
[Liu, F.] Univ Brussels, B-1050 Brussels, Belgium.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy.
[Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA.
[McGuire, S. C.; Vincent-Finley, R.] Southern Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.; Vincent-Finley, R.] A&M Coll, Baton Rouge, LA 70813 USA.
[Nayak, R.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Taejon 305390, South Korea.
[Raja, S.] RRCAT, Indore 452013, Madhya Pradesh, India.
[Rajalakshmi, G.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Mumbai 400005, Maharashtra, India.
[Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
[Reid, S.] Univ W Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland.
[Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
[Sengupta, A. S.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Vedovato, G.; Zendri, J. -P.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Williams, T.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
[Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
[Buchner, S.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa.
[Buchner, S.] Univ Witwatersrand, Sch Phys, Johannesburg, South Africa.
[Cognard, I.] Univ Orleans, LPC2E CNRS, F-45071 Orleans, France.
[Cognard, I.] Nancay Paris Observ, F-18330 Nancay, France.
[Corongiu, A.; D'Amico, N.; Possenti, A.] Osservatorio Astron Cagliari, INAF, I-09012 Poggio De Pini, Capoterra, Italy.
[D'Amico, N.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, Italy.
[Espinoza, C. M.; Kramer, M.; Lyne, A. G.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Espinoza, C. M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Freire, P. C. C.; Guillemot, L.; Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Hessels, J. W. T.] ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Hessels, J. W. T.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Hobbs, G. B.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Ray, P. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Roy, J.] Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI Ward, Robert/I-8032-2014; Cella, Giancarlo/A-9946-2012; Cesarini,
Elisabetta/C-4507-2017; 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; Harms,
Jan/J-4359-2012; Strain, Kenneth/D-5236-2011; Miao, Haixing/O-1300-2013;
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Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; Frasconi,
Franco/K-1068-2016; Groot, Paul/K-4391-2016; Pinto,
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Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo,
Michele/I-3995-2012; Puppo, Paola/J-4250-2012; Tacca,
Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Ottaway,
David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise,
Samuel/B-1599-2015; Neri, Igor/F-1482-2010; Shaddock,
Daniel/A-7534-2011; 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; Iyer, Bala
R./E-2894-2012; Canuel, Benjamin/C-7459-2014; Prokhorov,
Leonid/I-2953-2012; Lee, Chang-Hwan/B-3096-2015; Khalili,
Farit/D-8113-2012; Gorodetsky, Michael/C-5938-2008; McClelland,
David/E-6765-2010; M, Manjunath/N-4000-2014; Vecchio,
Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Strigin,
Sergey/I-8337-2012; Leonardi, Matteo/G-9694-2015; Sigg,
Daniel/I-4308-2015; Salemi, Francesco/F-6988-2014; Gammaitoni,
Luca/B-5375-2009; Bell, Angus/E-7312-2011; Nelemans, Gijs/D-3177-2012;
Kumar, Prem/B-6691-2009; prodi, giovanni/B-4398-2010; Gemme,
Gianluca/C-7233-2008; Costa, Cesar/G-7588-2012; Huerta,
Eliu/J-5426-2014; Losurdo, Giovanni/K-1241-2014; Steinlechner,
Sebastian/D-5781-2013; Hild, Stefan/A-3864-2010; Danilishin,
Stefan/K-7262-2012
OI Boschi, Valerio/0000-0001-8665-2293; Matichard,
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Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora
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prodi, giovanni/0000-0001-5256-915X; Gemme,
Gianluca/0000-0002-1127-7406; Losurdo, Giovanni/0000-0003-0452-746X;
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Stefan/0000-0001-7758-7493
FU United States National Science Foundation; Science and Technology
Facilities Council of the United Kingdom; Max-Planck-Society; State of
Niedersachsen/Germany; 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; 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; OTKA of Hungary; Lyon Institute of Origins (LIO);
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, OTKA of Hungary, the Lyon
Institute of Origins (LIO), the National Research Foundation of Korea,
Industry Canada and the Province of Ontario through the Ministry of
Economic Development and Innovation, the 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. The Nancay Radio
Observatory is operated by the Paris Observatory, associated with the
French Centre National de la Recherche Scientifique. LIGO Document No.
LIGO-P1200104.
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U1 6
U2 71
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2014
VL 785
IS 2
AR 119
DI 10.1088/0004-637X/785/2/119
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG9KA
UT WOS:000335736800038
ER
PT J
AU Bennett, DP
Batista, V
Bond, IA
Bennett, CS
Suzuki, D
Beaulieu, JP
Udalski, A
Donatowicz, J
Bozza, V
Abe, F
Botzler, CS
Freeman, M
Fukunaga, D
Fukui, A
Itow, Y
Koshimoto, N
Ling, CH
Masuda, K
Matsubara, Y
Muraki, Y
Namba, S
Ohnishi, K
Rattenbury, NJ
Saito, T
Sullivan, DJ
Sumi, T
Sweatman, WL
Tristram, PJ
Tsurumi, N
Wada, K
Yock, PCM
Albrow, MD
Bachelet, E
Brillant, S
Caldwell, JAR
Cassan, A
Cole, AA
Corrales, E
Coutures, C
Dieters, S
Prester, DD
Fouque, P
Greenhill, J
Horne, K
Koo, JR
Kubas, D
Marquette, JB
Martin, R
Menzies, JW
Sahu, KC
Wambsganss, J
Williams, A
Zub, M
Choi, JY
DePoy, DL
Dong, SB
Gaudi, BS
Gould, A
Han, C
Henderson, CB
McGregor, D
Lee, CU
Pogge, RW
Shin, IG
Yee, JC
Szymanski, MK
Skowron, J
Poleski, R
Kozllowski, S
Wyrzykowski, L
Kubiak, M
Pietrukowicz, P
Pietrzynski, G
Soszynski, I
Ulaczyk, K
Tsapras, Y
Street, RA
Dominik, M
Bramich, DM
Browne, P
Hundertmark, M
Kains, N
Snodgrass, C
Steele, IA
Dekany, I
Gonzalez, OA
Heyrovsky, D
Kandori, R
Kerins, E
Lucas, PW
Minniti, D
Nagayama, T
Rejkuba, M
Robin, AC
Saito, R
AF Bennett, D. P.
Batista, V.
Bond, I. A.
Bennett, C. S.
Suzuki, D.
Beaulieu, J. -P.
Udalski, A.
Donatowicz, J.
Bozza, V.
Abe, F.
Botzler, C. S.
Freeman, M.
Fukunaga, D.
Fukui, A.
Itow, Y.
Koshimoto, N.
Ling, C. H.
Masuda, K.
Matsubara, Y.
Muraki, Y.
Namba, S.
Ohnishi, K.
Rattenbury, N. J.
Saito, To.
Sullivan, D. J.
Sumi, T.
Sweatman, W. L.
Tristram, P. J.
Tsurumi, N.
Wada, K.
Yock, P. C. M.
Albrow, M. D.
Bachelet, E.
Brillant, S.
Caldwell, J. A. R.
Cassan, A.
Cole, A. A.
Corrales, E.
Coutures, C.
Dieters, S.
Prester, D. Dominis
Fouque, P.
Greenhill, J.
Horne, K.
Koo, J. -R.
Kubas, D.
Marquette, J. -B.
Martin, R.
Menzies, J. W.
Sahu, K. C.
Wambsganss, J.
Williams, A.
Zub, M.
Choi, J. Y.
DePoy, D. L.
Dong, Subo
Gaudi, B. S.
Gould, A.
Han, C.
Henderson, C. B.
McGregor, D.
Lee, C. -U.
Pogge, R. W.
Shin, I. -G.
Yee, J. C.
Szymanski, M. K.
Skowron, J.
Poleski, R.
Kozllowski, S.
Wyrzykowski, L.
Kubiak, M.
Pietrukowicz, P.
Pietrzynski, G.
Soszynski, I.
Ulaczyk, K.
Tsapras, Y.
Street, R. A.
Dominik, M.
Bramich, D. M.
Browne, P.
Hundertmark, M.
Kains, N.
Snodgrass, C.
Steele, I. A.
Dekany, I.
Gonzalez, O. A.
Heyrovsky, D.
Kandori, R.
Kerins, E.
Lucas, P. W.
Minniti, D.
Nagayama, T.
Rejkuba, M.
Robin, A. C.
Saito, R.
CA MOA Collaboration
PLANET Collaboration
FUN Collaboration
OGLE Collaboration
RoboNet Collaboration
TI MOA-2011-BLG-262Lb: A SUB-EARTH-MASS MOON ORBITING A GAS GIANT PRIMARY
OR A HIGH VELOCITY PLANETARY SYSTEM IN THE GALACTIC BULGE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing: micro; planetary systems
ID GRAVITATIONAL LENSING EXPERIMENT; FREE-FLOATING PLANET; MAGNIFICATION
MICROLENSING EVENTS; SNOW LINE; EXTRASOLAR PLANETS; MAIN-SEQUENCE;
STELLAR-MASS; BROWN DWARF; OGLE-III; JUPITER/SATURN ANALOG
AB We present the first microlensing candidate for a free-floating exoplanet-exomoon system, MOA-2011-BLG-262, with a primary lens mass of M-host similar to 4 Jupitermasses hosting a sub-Earthmassmoon. The argument for an exomoon hinges on the system being relatively close to the Sun. The data constrain the product M-L pi(rel) where ML is the lens system mass and prel is the lens-source relative parallax. If the lens system is nearby (large pi(rel)), then ML is small (a few Jupiter masses) and the companion is a sub-Earth-mass exomoon. The best-fit solution has a large lens-source relative proper motion, mu(rel) = 19.6 +/- 1.6 mas yr(-1), which would rule out a distant lens system unless the source star has an unusually high proper motion. However, data from the OGLE collaboration nearly rule out a high source proper motion, so the exoplanet+exomoon model is the favored interpretation for the best fit model. However, there is an alternate solution that has a lower proper motion and fits the data almost as well. This solution is compatible with a distant (so stellar) host. A Bayesian analysis does not favor the exoplanet+exomoon interpretation, so Occam's razor favors a lens system in the bulge with host and companion masses of M-host = 0.12(-0.06)(+0.19) M-circle dot and m(comp) = 18(-10)(+28) M-circle plus, at a projected separation of a(perpendicular to) = 0.84(-0.14)(+0.25) AU. The existence of this degeneracy is an unlucky accident, so current microlensing experiments are in principle sensitive to exomoons. In some circumstances, it will be possible to definitively establish the mass of such lens systems through the microlensing parallax effect. Future experiments will be sensitive to less extreme exomoons.
C1 [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Batista, V.; Gaudi, B. S.; Gould, A.; McGregor, D.; Pogge, R. W.; Yee, J. C.; Poleski, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Batista, V.; Beaulieu, J. -P.; Cassan, A.; Corrales, E.; Coutures, C.; Kubas, D.; Marquette, J. -B.] UPMC, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Bond, I. A.; Ling, C. H.; Sweatman, W. L.] Massey Univ, Inst Nat & Math Sci, Auckland 0745, New Zealand.
[Bennett, C. S.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Bennett, C. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Suzuki, D.; Koshimoto, N.; Namba, S.; Sumi, T.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Udalski, A.; Szymanski, M. K.; Skowron, J.; Poleski, R.; Kozllowski, S.; Wyrzykowski, L.; Kubiak, M.; Pietrukowicz, P.; Pietrzynski, G.; Soszynski, I.; Ulaczyk, K.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Donatowicz, J.] Vienna Univ Technol, A-1040 Vienna, Austria.
[Bozza, V.] Univ Salerno, Dipartimento Fis, I-84084 Fisciano, Italy.
[Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy.
[Abe, F.; Fukunaga, D.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Tsurumi, N.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Botzler, C. S.; Freeman, M.; Rattenbury, N. J.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand.
[Fukui, A.] Natl Astron Observ, Okayama Astrophys Observ, Okayama 7190232, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, To.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan.
[Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington 6140, New Zealand.
[Tristram, P. J.] Mt John Univ Observ, Lake Tekapo 8770, New Zealand.
[Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand.
[Bachelet, E.; Fouque, P.] Univ Toulouse, CNRS, IRAP, F-31400 Toulouse, France.
[Brillant, S.; Gonzalez, O. A.; Rejkuba, M.] European So Observ, Santiago 19, Chile.
[Caldwell, J. A. R.] McDonald Observ, Fort Davis, TX 79734 USA.
[Cole, A. A.; Dieters, S.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Prester, D. Dominis] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia.
[Horne, K.; Dominik, M.; Browne, P.; Hundertmark, M.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Koo, J. -R.; Choi, J. Y.; Han, C.; Shin, I. -G.] Chungbuk Natl Univ, Dept Phys, Chongju 371763, South Korea.
[Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia.
[Menzies, J. W.] S African Astron Observ, ZA-7925 Cape Town, South Africa.
[Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Wambsganss, J.; Zub, M.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany.
[DePoy, D. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Tsapras, Y.; Street, R. A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Tsapras, Y.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England.
[Bramich, D. M.; Kains, N.] ESO Headquarters, D-85748 Munich, Germany.
[Bramich, D. M.] Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar.
[Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England.
[Dekany, I.; Minniti, D.; Saito, R.] Pontificia Univ Catolica Chile, Santiago 22, Chile.
[Heyrovsky, D.] Charles Univ Prague, Inst Theoret Phys, Prague 18000, Czech Republic.
[Kandori, R.; Nagayama, T.] Nagoya Univ, Grad Sch Sci, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Kerins, E.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Lucas, P. W.] Univ Hertfordshire, Hatfield AL10 9AB, Herts, England.
[Robin, A. C.] Univ Franche Comte, UTINAM, CNRS, Observ Besancon Inst,UMR 6213, F-25010 Besancon, France.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Bennett, DP (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA.
EM bennett@nd.edu
RI Skowron, Jan/M-5186-2014; Heyrovsky, David/A-2031-2015; Williams,
Andrew/K-2931-2013; Hundertmark, Markus/C-6190-2015; Saito,
Roberto/L-6722-2016;
OI Skowron, Jan/0000-0002-2335-1730; Heyrovsky, David/0000-0002-5198-5343;
Williams, Andrew/0000-0001-9080-0105; Hundertmark,
Markus/0000-0003-0961-5231; Dominik, Martin/0000-0002-3202-0343; Cole,
Andrew/0000-0003-0303-3855; Rejkuba, Marina/0000-0002-6577-2787;
Snodgrass, Colin/0000-0001-9328-2905
FU JSPS [JSPS23340044, JSPS24253004]; NASA Keck PI Data Award; W. M. Keck
Foundation; NSF [AST 110347, AST-0807444]; NASA [NNX12AB99G]; Ralph E.
and Doris M. Hansmann Membership at the IAS; California Institute of
Technology (Caltech); NASA through the Sagan Fellowship Program;
European Research Council under the European Community's Seventh
Framework Programme (FP7)/ERC [246678]; Czech Science Foundation grant
GACR [P209/10/1318]; NPRP grant from the Qatar National Research Fund (a
member of the Qatar Foundation) [NPRP-09-476-1-78]; [NASA-NNX12AF54G];
[JPL-RSA 1453175]; [NSF AST-1211875]; [JSPS18253002]; [JSPS20340052]
FX D.P.B. was supported by grants NASA-NNX12AF54G, JPL-RSA 1453175 and NSF
AST-1211875. This MOA project is supported by the grants JSPS18253002
and JSPS20340052. T. S. acknowledges the financial support from the
JSPS, JSPS23340044, JSPS24253004. This work was partially supported by a
NASA Keck PI Data Award, administered by the NASA Exoplanet Science
Institute. Data presented herein were obtained at the W. M. Keck
Observatory from telescope time allocated to the National Aeronautics
and Space Administration through the agency's scientific partnership
with the California Institute of Technology and the University of
California. The Observatory was made possible by the generous financial
support of the W. M. Keck Foundation. B. S. G. and A. G. were supported
by NSF grant AST 110347. B. S. G., A. G., R. P. G. were supported by
NASA grant NNX12AB99G. S. D. was partly supported through a Ralph E. and
Doris M. Hansmann Membership at the IAS and by NSF grant AST-0807444.
Work by J.C.Y. was performed in part under contract with the California
Institute of Technology (Caltech) funded by NASA through the Sagan
Fellowship Program. The OGLE project has received funding from the
European Research Council under the European Community's Seventh
Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A.
U. D. H. was supported by Czech Science Foundation grant GACR
P209/10/1318. D. M. B., M. D., K. H., C. S., R. A. S., M. H. and Y.T.
are supported by NPRP grant NPRP-09-476-1-78 from the Qatar National
Research Fund (a member of the Qatar Foundation).
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA AG9KA
UT WOS:000335736800074
ER
PT J
AU Kane, SR
Howell, SB
Horch, EP
Feng, Y
Hinkel, NR
Ciardi, DR
Everett, ME
Howard, AW
Wright, JT
AF Kane, Stephen R.
Howell, Steve B.
Horch, Elliott P.
Feng, Ying
Hinkel, Natalie R.
Ciardi, David R.
Everett, Mark E.
Howard, Andrew W.
Wright, Jason T.
TI LIMITS ON STELLAR COMPANIONS TO EXOPLANET HOST STARS WITH ECCENTRIC
PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (HD 4203, HD 168443, HD 1690, HD
137759); techniques: high angular resolution; techniques: radial
velocities
ID SOLAR-TYPE STARS; GIANT IOTA-DRACONIS; BINARY STARS; STATISTICAL
PROPERTIES; REFRACTORY ELEMENTS; EXTRASOLAR PLANETS; HIPPARCOS STARS;
MULTIPLICITY; ABUNDANCES; DISCOVERY
AB Though there are now many hundreds of confirmed exoplanets known, the binarity of exoplanet host stars is not well understood. This is particularly true of host stars that harbor a giant planet in a highly eccentric orbit since these are more likely to have had a dramatic dynamical history that transferred angular momentum to the planet. Here we present observations of four exoplanet host stars that utilize the excellent resolving power of the Differential Speckle Survey Instrument on the Gemini North telescope. Two of the stars are giants and two are dwarfs. Each star is host to a giant planet with an orbital eccentricity >0.5 and whose radial velocity (RV) data contain a trend in the residuals to the Keplerian orbit fit. These observations rule out stellar companions 4-8 mag fainter than the host star at passbands of 692 nm and 880 nm. The resolution and field of view of the instrument result in exclusion radii of 0.'' 05-1.'' 4, which excludes stellar companions within several AU of the host star in most cases. We further provide new RVs for the HD 4203 system that confirm that the linear trend previously observed in the residuals is due to an additional planet. These results place dynamical constraints on the source of the planet's eccentricities, place constraints on additional planetary companions, and inform the known distribution of multiplicity amongst exoplanet host stars.
C1 [Kane, Stephen R.; Hinkel, Natalie R.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA.
[Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
[Feng, Ying; Wright, Jason T.] Penn State Univ, Dept Phys & Astron, University Pk, PA 16802 USA.
[Feng, Ying; Wright, Jason T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Kane, SR (reprint author), San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA.
EM skane@sfsu.edu
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Wright, Jason/0000-0001-6160-5888;
Ciardi, David/0000-0002-5741-3047
FU National Aeronautics and Space Administration; National Science
Foundation [AST-1109662]
FX This work is based on observations obtained at the Gemini Observatory,
which is operated by the Association of Universities for Research in
Astronomy, Inc., under a cooperative agreement with the NSF on behalf of
the Gemini partnership: the National Science Foundation (United States),
the National Research Council (Canada), CONICYT (Chile), the Australian
Research Council (Australia), Ministerio da Ciencia, Tecnologia e
Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion
Productiva (Argentina). This research has made use of the Exoplanet
Orbit Database and the Exoplanet Data Explorer at exoplanets.org. This
research has also made use of the NASA/IPAC Infrared Science Archive,
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under contract with the National Aeronautics and Space
Administration. The authors acknowledge financial support from the
National Science Foundation through grant AST-1109662.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA AG9KA
UT WOS:000335736800012
ER
PT J
AU Kataria, T
Showman, AP
Fortney, JJ
Marley, MS
Freedman, RS
AF Kataria, T.
Showman, A. P.
Fortney, J. J.
Marley, M. S.
Freedman, R. S.
TI THE ATMOSPHERIC CIRCULATION OF THE SUPER EARTH GJ 1214b: DEPENDENCE ON
COMPOSITION AND METALLICITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atmospheric effects; methods: numerical; planets and satellites:
atmospheres; planets and satellites: composition; planets and
satellites: individual (GJ 1214b)
ID HOT JUPITERS; TRANSMISSION SPECTRUM; HD 209458B; EXOPLANET; MODEL;
SPECTROSCOPY; DYNAMICS; NEPTUNE; GJ1214B; CLOUDS
AB We present three-dimensional atmospheric circulation models of GJ 1214b, a 2.7 Earth-radius, 6.5 Earth-mass super Earth detected by the MEarth survey. Here we explore the planet's circulation as a function of atmospheric metallicity and atmospheric composition, modeling atmospheres with a low mean molecular weight (MMW; i.e., H-2-dominated) and a high MMW (i.e., water-and CO2-dominated). We find that atmospheres with a low MMW have strong day-night temperature variations at pressures above the infrared photosphere that lead to equatorial superrotation. For these atmospheres, the enhancement of atmospheric opacities with increasing metallicity lead to shallower atmospheric heating, larger day-night temperature variations, and hence stronger superrotation. In comparison, atmospheres with a high MMW have larger day-night and equator-to-pole temperature variations than low MMW atmospheres, but differences in opacity structure and energy budget lead to differences in jet structure. The circulation of a water-dominated atmosphere is dominated by equatorial superrotation, while the circulation of a CO2-dominated atmosphere is instead dominated by high-latitude jets. By comparing emergent flux spectra and light curves for 50x solar and water-dominated compositions, we show that observations in emission can break the degeneracy in determining the atmospheric composition of GJ 1214b. The variation in opacity with wavelength for the water-dominated atmosphere leads to large phase variations within water bands and small phase variations outside of water bands. The 50x solar atmosphere, however, yields small variations within water bands and large phase variations at other characteristic wavelengths. These observations would be much less sensitive to clouds, condensates, and hazes than transit observations.
C1 [Kataria, T.; Showman, A. P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Kataria, T.; Showman, A. P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Marley, M. S.; Freedman, R. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Freedman, R. S.] SETI Inst, Mountain View, CA 94043 USA.
RP Kataria, T (reprint author), Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
EM tkataria@lpl.arizona.edu
RI Marley, Mark/I-4704-2013;
OI Fortney, Jonathan/0000-0002-9843-4354; Marley, Mark/0000-0002-5251-2943
FU Origins grant [NNX12AI79G]; Harriet P. Jenkins Pre-Doctoral Fellowship
Program (JPFP); NASA High-End Computing (HEC) Program through the NASA
Advanced Supercomputing (NAS) Division at Ames Research Center
FX This work was supported by Origins grant NNX12AI79G to A.P.S. T.K. also
acknowledges support from the Harriet P. Jenkins Pre-Doctoral Fellowship
Program (JPFP). 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. We thank Roxana
Lupu for comments and for providing opacity tables for
CO2-CO2 pressure-induced absorption. We also thank
Daniel Apai, Nikole Lewis, and Robert Zellem for insightful discussions.
Last, we thank the anonymous referee for helpful comments and
suggestions.
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UT WOS:000335736800011
ER
PT J
AU Lau, RM
Herter, TL
Morris, MR
Adams, JD
AF Lau, R. M.
Herter, T. L.
Morris, M. R.
Adams, J. D.
TI NATURE VERSUS NURTURE: LUMINOUS BLUE VARIABLE NEBULAE IN AND NEAR
MASSIVE STELLAR CLUSTERS AT THE GALACTIC CENTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: center; Hii regions; Infrared: ISM; stars: evolution
ID PASCHEN-ALPHA SURVEY; WOLF-RAYET STARS; QUINTUPLET CLUSTER;
TEMPERATURE-FLUCTUATIONS; OPTICAL-PROPERTIES; MAGNETIC-FIELD; SMALL
GRAINS; DUST; PISTOL; SPECTROSCOPY
AB Three luminous blue variables (LBVs) are located in and near the Quintuplet Cluster at the Galactic center: the Pistol Star, G0.120-0.048, and qF362. We present imaging at 19, 25, 31, and 37 mu m of the region containing these three LBVs, obtained with SOFIA using FORCAST. We argue that Pistol and G0.120-0.048 are identical " twins" that exhibit contrasting nebulae due to the external influence of their different environments. Our images reveal the asymmetric, compressed shell of hot dust surrounding the Pistol Star and provide the first detection of the thermal emission from the symmetric, hot dust envelope surrounding G0.120-0.048. However, no detection of hot dust associated with qF362 is made. Dust and gas composing the Pistol nebula are primarily heated and ionized by the nearby Quintuplet Cluster stars. The northern region of the Pistol nebula is decelerated due to the interactionwith the high-velocity (2000 km s(-1)) winds from adjacent Wolf-Rayet Carbon (WC) stars. From fits to the spectral energy distribution (SED) of the Pistol nebula with the DustEM code we determine that the Pistol nebula is composed of a distribution of very small, transiently heated grains (10 to similar to 35 angstrom) having a total dust mass of 0.03M(circle dot), and that it exhibits a gradient of decreasing grain size from south to north due to differential sputtering by the winds from the WC stars. The total IR luminosity of the Pistol nebula is 5.2 x 10 (5) L-circle dot. Dust in the G0.120-0.048 nebula is primarily heated by the central star; however, the nebular gas is ionized externally by the Arches Cluster. Unlike the Pistol nebula, the G0.120-0.048 nebula is freely expanding into the surrounding medium. A grain size distribution identical to that of the non-sputtered region of the Pistol nebula satisfies the constraints placed on the G0.120-0.048 nebula from DustEM model fits to its SED and implies a total dust mass of 0.021M(circle dot). The total IR luminosity of the G0.120-0.048 nebula is similar to 10(5) L-circle dot. From Paschen-alpha and 6 cm observations we determine a total gas mass of 9.3M(circle dot) and 6.2M(circle dot) for the Pistol and G0.120-0.048 nebulae, respectively. Given the independent dust and gas mass estimates we find that the Pistol and G0.120-0.048 nebulae exhibit similar gas-to-dust mass ratios of 310+ 77 -52 and 293+ 73 -101, respectively. Both nebulae share identical size scales (similar to 0.7 pc) which suggests that they have similar dynamical timescales of similar to 10(4) yr, assuming a shell expansion velocity of vexp = 60 km s(-1).
C1 [Lau, R. M.; Herter, T. L.; Adams, J. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Morris, M. R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Adams, J. D.] NASA, Ames Res Ctr, Univ Space Res Assoc, 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 [NAS2-97001, 8500-98-014]; Deutsches SOFIA Institut (DSI) under DLR
[50 OK 0901]; USRA
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. 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 50 OK 0901. Financial support for FORCAST was
provided by NASA through award 8500-98-014 issued by USRA.
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SC Astronomy & Astrophysics
GA AG9KA
UT WOS:000335736800039
ER
PT J
AU Lis, DC
Schilke, P
Bergin, EA
Gerin, M
Black, JH
Comito, C
De Luca, M
Godard, B
Higgins, R
Le Petit, F
Pearson, JC
Pellegrini, EW
Phillips, TG
Yu, S
AF Lis, D. C.
Schilke, P.
Bergin, E. A.
Gerin, M.
Black, J. H.
Comito, C.
De Luca, M.
Godard, B.
Higgins, R.
Le Petit, F.
Pearson, J. C.
Pellegrini, E. W.
Phillips, T. G.
Yu, S.
TI WIDESPREAD ROTATIONALLY HOT HYDRONIUM ION IN THE GALACTIC INTERSTELLAR
MEDIUM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; galaxies: nuclei; ISM: molecules; molecular processes;
submillimeter: general; techniques: spectroscopic
ID SIGHT-LINE; SGR B2; MOLECULAR-HYDROGEN; H3O+; AMMONIA; CLOUDS; REGIONS;
HIFI; H2O+; GAS
AB We present new Herschel observations of the (6,6) and (9,9) inversion transitions of the hydronium ion toward Sagittarius B2(N) and W31C. Sensitive observations toward Sagittarius B2(N) show that the high, similar to 500 K, rotational temperatures characterizing the population of the highly excited metastable H3O+ rotational levels are present over a wide range of velocities corresponding to the Sagittarius B2 envelope, as well as the foreground gas clouds between the Sun and the source. Observations of the same lines toward W31C, a line of sight that does not intersect the Central Molecular Zone but instead traces quiescent gas in the Galactic disk, also imply a high rotational temperature of similar to 380 K, well in excess of the kinetic temperature of the diffuse Galactic interstellar medium. While it is plausible that some fraction of the molecular gas may be heated to such high temperatures in the active environment of the Galactic center, characterized by high X-ray and cosmic-ray fluxes, shocks, and high degree of turbulence, this is unlikely in the largely quiescent environment of the Galactic disk clouds. We suggest instead that the highly excited states of the hydronium ion are populated mainly by exoergic chemical formation processes and the temperature describing the rotational level population does not represent the physical temperature of the medium. The same arguments may be applicable to other symmetric top rotors, such as ammonia. This offers a simple explanation of the long-standing puzzle of the presence of a pervasive, hot molecular gas component in the central region of the Milky Way. Moreover, our observations suggest that this is a universal process not limited to the active environments associated with galactic nuclei.
C1 [Lis, D. C.; Phillips, T. G.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA.
[Lis, D. C.] Univ Paris 06, Sorbonne Univ, CNRS, Observ Paris,LERMA,UMR 8112, Paris, France.
[Schilke, P.; Comito, C.; Higgins, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
[Bergin, E. A.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Gerin, M.; De Luca, M.; Godard, B.; Le Petit, F.] Ecole Normale Super, CNRS, Observ Paris, LERMA,UMR 8112, Paris, France.
[Black, J. H.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
[Pearson, J. C.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Pellegrini, E. W.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
RP Lis, DC (reprint author), CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA.
EM dcl@caltech.edu; schilke@ph1.uni-koeln.de; ebergin@umich.edu;
maryvonne.gerin@lra.ens.fr; john.black@chalmers.se;
ccomito@ph1.uni-koeln.de; deluca@lra.ens.fr; benjamin.godard@lra.ens.fr;
higgins@ph1.uni-koeln.de; franck.lepetit@obspm.fr;
john.c.pearson@jpl.nasa.gov; eric.pellegrini@utoledo.edu;
tgp@submm.caltech.edu; shanshan.yu@jpl.nasa.gov
RI Yu, Shanshan/D-8733-2016
FU NASA through JPL/Caltech; Collaborative Research Center 956 - Deutsche
Forschungsgemeinschaft (DFG)
FX HIFI has been designed and built by a consortium of institutes and
university departments from across Europe, Canada, and the United States
(NASA) under the leadership of SRON, Netherlands Institute for Space
Research, Groningen, The Netherlands, and with major contributions from
Germany, France, and the US. Support for this work was provided by NASA
(Herschel OT funding) through an award issued by JPL/Caltech. The
research of P. S., C. C., and R. H. is supported by the Collaborative
Research Center 956 funded by the Deutsche Forschungsgemeinschaft (DFG).
NR 46
TC 11
Z9 11
U1 1
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 APR 20
PY 2014
VL 785
IS 2
AR 135
DI 10.1088/0004-637X/785/2/135
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG9KA
UT WOS:000335736800054
ER
PT J
AU Masters, D
McCarthy, P
Siana, B
Malkan, M
Mobasher, B
Atek, H
Henry, A
Martin, CL
Rafelski, M
Hathi, NP
Scarlata, C
Ross, NR
Bunker, AJ
Blanc, G
Bedregal, AG
Dominguez, A
Colbert, J
Teplitz, H
Dressler, A
AF Masters, Daniel
McCarthy, Patrick
Siana, Brian
Malkan, Mathew
Mobasher, Bahram
Atek, Hakim
Henry, Alaina
Martin, Crystal L.
Rafelski, Marc
Hathi, Nimish P.
Scarlata, Claudia
Ross, Nathaniel R.
Bunker, Andrew J.
Blanc, Guillermo
Bedregal, Alejandro G.
Dominguez, Alberto
Colbert, James
Teplitz, Harry
Dressler, Alan
TI PHYSICAL PROPERTIES OF EMISSION-LINE GALAXIES AT z similar to 2 FROM
NEAR-INFRARED SPECTROSCOPY WITH MAGELLAN FIRE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: abundances; galaxies: high-redshift; galaxies: kinematics and
dynamics; galaxies: starburst; galaxies: star formation
ID STAR-FORMING GALAXIES; MASS-METALLICITY RELATION; H-II REGIONS; DIGITAL
SKY SURVEY; INTEGRAL FIELD SPECTROSCOPY; FRAME OPTICAL-SPECTRA; LYMAN
BREAK GALAXIES; GREATER-THAN 1; HIGH-REDSHIFT; CHEMICAL ABUNDANCES
AB We present results from near-infrared spectroscopy of 26 emission-line galaxies at z similar to 2.2 and z similar to 1.5 obtained with the Folded-port InfraRed Echellette (FIRE) spectrometer on the 6.5 m Magellan Baade telescope. The sample was selected from the WFC3 Infrared Spectroscopic Parallels survey, which uses the near-infrared grism of the Hubble Space Telescope Wide Field Camera 3 (WFC3) to detect emission-line galaxies over 0.3 less than or similar to z less than or similar to 2.3. Our FIRE follow-up spectroscopy (R similar to 5000) over 1.0-2.5 mu m permits detailedmeasurements of the physical properties of the z similar to 2 emission-line galaxies. Dust-corrected star formation rates for the sample range from similar to 5-100 M-circle dot yr(-1) with a mean of 29 M-circle dot yr(-1). We derive a median metallicity for the sample of 12 + log(O/H) = 8.34 or similar to 0.45 Z(circle dot). The estimated stellar masses range from similar to 10(8.5)-10(9.5) M-circle dot, and a clear positive correlation between metallicity and stellar mass is observed. The average ionization parameter measured for the sample, log U approximate to -2.5, is significantly higher than what is found for most star-forming galaxies in the local universe, but similar to the values found for other star-forming galaxies at high redshift. We derive composite spectra from the FIRE sample, from which we measure typical nebular electron densities of similar to 100-400 cm(-3). Based on the location of the galaxies and composite spectra on diagnostic diagrams, we do not find evidence for significant active galactic nucleus activity in the sample. Most of the galaxies, as well as the composites, are offset diagram toward higher [O III]/H beta at a given [N II]/H alpha, in agreement with other observations of z greater than or similar to 1 star-forming galaxies, but composite spectra derived from the sample do not show an appreciable offset from the local star-forming sequence on the [O III]/H beta versus [S II]/H alpha diagram. We infer a high nitrogen-to-oxygen abundance ratio from the composite spectrum, which may contribute to the offset of the high-redshift galaxies from the local star-forming sequence in the [O III]/H beta versus [N II]/H alpha diagram. We speculate that the elevated nitrogen abundance could result from substantial numbers of Wolf-Rayet stars in starbursting galaxies at z similar to 2.
C1 [Masters, Daniel; Siana, Brian; Mobasher, Bahram; Dominguez, Alberto] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Masters, Daniel; McCarthy, Patrick; Blanc, Guillermo; Dressler, Alan] Carnegie Observ, Pasadena, CA 91101 USA.
[Malkan, Mathew; Ross, Nathaniel R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Atek, Hakim] Ecole Polytech Fed, Astrophys Lab, CH-1290 Sauverny, Switzerland.
[Henry, Alaina] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Martin, Crystal L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Rafelski, Marc; Colbert, James] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Hathi, Nimish P.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Scarlata, Claudia] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Bunker, Andrew J.] Univ Oxford, Dept Phys, Oxford OX1 2JD, England.
[Bedregal, Alejandro G.] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA.
[Teplitz, Harry] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
RP Masters, D (reprint author), Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
RI Blanc, Guillermo/I-5260-2016; Hathi, Nimish/J-7092-2014;
OI Hathi, Nimish/0000-0001-6145-5090; Dominguez,
Alberto/0000-0002-3433-4610
FU Carnegie Observatories graduate research fellowship; NSF [AAG 1109288]
FX We thank the anonymous referee for thoughtful comments and suggestions
that significantly improved this paper, and Evan Skillman for a careful
reading and helpful comments. We are also grateful to Rob Simcoe, Lisa
Kewley, Ryan Quadri, Daniel Kelson, and Louis Abramson for discussions
regarding the FIRE observations and science. D. C. M. gratefully
acknowledges the support provided by the Carnegie Observatories graduate
research fellowship, as well as the excellent support provided by the
staff of the Las Campanas Observatory. C. L. M. acknowledges support
from NSF AAG 1109288.
NR 96
TC 59
Z9 59
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2014
VL 785
IS 2
AR 153
DI 10.1088/0004-637X/785/2/153
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG9KA
UT WOS:000335736800072
ER
PT J
AU Nakamura, M
Meier, DL
AF Nakamura, Masanori
Meier, David L.
TI A MAGNETOHYDRODYNAMIC MODEL OF THE M87 JET. II. SELF-CONSISTENT
QUAD-SHOCK JET MODEL FOR OPTICAL RELATIVISTIC MOTIONS AND PARTICLE
ACCELERATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (M87); galaxies: jets;
magnetohydrodynamics (MHD); methods: numerical
ID COSMIC-RAY ACCELERATION; HUBBLE-SPACE-TELESCOPE; MAGNETIC-FIELD
AMPLIFICATION; ACTIVE GALACTIC NUCLEI; BASE-LINE ARRAY;
ULTRARELATIVISTIC SHOCKS; NUMERICAL SIMULATIONS; ASTROPHYSICAL SHOCKS;
FERMI ACCELERATION; INTERNAL SHOCKS
AB We describe a new paradigm for understanding both relativistic motions and particle acceleration in the M87 jet: a magnetically dominated relativistic flow that naturally produces four relativistic magnetohydrodynamic (MHD) shocks (forward/reverse fast and slow modes). We apply this model to a set of optical super-and subluminal motions discovered by Biretta and coworkers with the Hubble Space Telescope during 1994-1998. The model concept consists of ejection of a single relativistic Poynting jet, which possesses a coherent helical (poloidal + toroidal) magnetic component, at the remarkably flaring point HST-1. We are able to reproduce quantitatively proper motions of components seen in the optical observations of HST-1 with the same model we used previously to describe similar features in radio very long baseline interferometry observations in 2005-2006. This indicates that the quad relativistic MHD shock model can be applied generally to recurring pairs of super/subluminal knots ejected from the upstream edge of the HST-1 complex as observed from radio to optical wavelengths, with forward/reverse fast-mode MHD shocks then responsible for observed moving features. Moreover, we identify such intrinsic properties as the shock compression ratio, degree of magnetization, and magnetic obliquity and show that they are suitable to mediate diffusive shock acceleration of relativistic particles via the first-order Fermi process. We suggest that relativistic MHD shocks in Poynting-flux-dominated helical jets may play a role in explaining observed emission and proper motions in many active galactic nuclei.
C1 [Nakamura, Masanori] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Meier, David L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nakamura, M (reprint author), Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS-NTU 1, Taipei 10617, Taiwan.
EM nakamura@asiaa.sinica.edu.tw; david.l.meier@jpl.nasa.gov
FU Allan C. Davis fellowship; Department of Physics and Astronomy at Johns
Hopkins University; Space Telescope Science Institute; National
Aeronautics and Space Administration
FX M.N. acknowledges part of this research was carried out under supported
by the Allan C. Davis fellowship jointly awarded by the Department of
Physics and Astronomy at Johns Hopkins University and the Space
Telescope Science Institute. Part of this research also was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under contract with the National Aeronautics and Space Administration.
NR 60
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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 APR 20
PY 2014
VL 785
IS 2
AR 152
DI 10.1088/0004-637X/785/2/152
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG9KA
UT WOS:000335736800071
ER
PT J
AU Ranjan, S
Charbonneau, D
Desert, JM
Madhusudhan, N
Deming, D
Wilkins, A
Mandell, AM
AF Ranjan, Sukrit
Charbonneau, David
Desert, Jean-Michel
Madhusudhan, Nikku
Deming, Drake
Wilkins, Ashlee
Mandell, Avi M.
TI ATMOSPHERIC CHARACTERIZATION OF FIVE HOT JUPITERS WITH THE WIDE FIELD
CAMERA 3 ON THE HUBBLE SPACE TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; planetary systems; techniques: photometric; techniques:
spectroscopic
ID NICMOS TRANSMISSION SPECTROSCOPY; EXTRASOLAR PLANET ATMOSPHERE;
COLLISION-INDUCED ABSORPTION; INFRARED-EMISSION SPECTRUM; SECONDARY
ECLIPSE; HD 189733B; TEMPERATURE INVERSION; EXOPLANET ATMOSPHERES; MODEL
ATMOSPHERES; THERMAL EMISSION
AB We probe the structure and composition of the atmospheres of five hot Jupiter exoplanets using the Hubble Space Telescope Wide Field Camera 3 (WFC3) instrument. We use the G141 grism (1.1-1.7 mu m) to study TrES-2b, TrES-4b, and CoRoT-1b in transit; TrES-3b in secondary eclipse; and WASP-4b in both. This wavelength region includes a predicted absorption feature from water at 1.4 mu m, which we expect to be nondegenerate with the other molecules that are likely to be abundant for hydrocarbon-poor (e. g., solar composition) hot Jupiter atmospheres. We divide our wavelength regions into 10 bins. For each bin we produce a spectrophotometric light curve spanning the time of transit or eclipse. We correct these light curves for instrumental systematics without reference to an instrument model. For our transmission spectra, our mean 1 sigma precision per bin corresponds to variations of 2.1, 2.8, and 3.0 atmospheric scale heights for TrES-2b, TrES-4b, and CoRoT-1b, respectively. We find featureless spectra for these three planets. We are unable to extract a robust transmission spectrum for WASP-4b. For our dayside emission spectra, our mean 1 sigma precision per bin corresponds to a planet-to-star flux ratio of 1.5 x 10(-4) and 2.1 x 10(-4) for WASP-4b and TrES-3b, respectively. We combine these estimates with previous broadband measurements and conclude that for both planets isothermal atmospheres are disfavored. We find no signs of features due to water. We confirm that WFC3 is suitable for studies of transiting exoplanets, but in staring mode multivisit campaigns are necessary to place strong constraints on water abundance.
C1 [Ranjan, Sukrit; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Desert, Jean-Michel] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Madhusudhan, Nikku] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA.
[Deming, Drake; Wilkins, Ashlee] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mandell, Avi M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Desert, Jean-Michel] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
RP Ranjan, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM sranjan@cfa.harvard.edu
OI Ranjan, Sukrit/0000-0002-5147-9053
FU NASA through Space Telescope Science Institute; NASA [NAS 5-26555];
National Science Foundation Graduate Research Fellowship [DGE-1144152];
California Institute of Technology (Caltech); NASA through the Sagan
Fellowship Program grant; Yale University through the YCAA postdoctoral
prize fellowship; [HST-GO-12181]
FX Based on observations made with the NASA/ESA Hubble Space Telescope,
obtained at the Space Telescope Science Institute (STScI). These
observations are associated with program HST-GO-12181. Support for this
program was provided by NASA through a grant from the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This
material is based upon work supported by the National Science Foundation
Graduate Research Fellowship under grant No. DGE-1144152. This work was
also performed in part under contract with the California Institute of
Technology (Caltech) funded by NASA through the Sagan Fellowship Program
grant awarded to J.-M.D. N.M. acknowledges support from Yale University
through the YCAA postdoctoral prize fellowship. This research has made
use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at
exoplanets.org; the SIMBAD database, operated at CDS, Strasbourg,
France; NASA's Astrophysics Data System Bibliographic Services; and
SAOImage DS9, developed by Smithsonian Astrophysical Observatory. The
authors are grateful to Z. Berta-Thompson and J. Carter for many
fruitful discussions, to the STScI HST help team for their assistance,
and to an anonymous referee whose comments strengthened the paper.
NR 69
TC 15
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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
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2014
VL 785
IS 2
AR 148
DI 10.1088/0004-637X/785/2/148
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG9KA
UT WOS:000335736800067
ER
PT J
AU Robinson, TD
Marley, MS
AF Robinson, Tyler D.
Marley, Mark S.
TI TEMPERATURE FLUCTUATIONS AS A SOURCE OF BROWN DWARF VARIABILITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; convection; radiation mechanisms: thermal; stars:
atmospheres
ID LOW-MASS STARS; T-DWARFS; EVOLVING WEATHER; ULTRACOOL DWARFS; INFRARED
COLORS; GRAVITY-WAVES; GIANT PLANETS; ATMOSPHERES; MODELS; CLOUDS
AB A number of brown dwarfs are now known to be variable with observed amplitudes as large as 10%-30% at some wavelengths. While spatial inhomogeneities in cloud coverage and thickness are likely responsible for much of the observed variability, it is possible that some of the variations arise from atmospheric temperature fluctuations instead of, or in addition to, clouds. To better understand the role that thermal variability might play we present a case study of brown dwarf variability using a newly developed one-dimensional, time-stepping model of atmospheric thermal structure. We focus on the effects of thermal perturbations, intentionally simplifying the problem through omission of clouds and atmospheric circulation. Model results demonstrate that thermal perturbations occurring deep in the atmosphere (at pressures greater than 10 bar) of a model T-dwarf can be communicated to the upper atmosphere through radiative heating via the windows in near-infrared water opacity. The response time depends on where in the atmosphere a thermal perturbation is introduced. We show that, for certain periodic perturbations, the emission spectrum can have complex time-and wavelength-dependent behaviors, including phase shifts in times of maximum flux observed at different wavelengths. Since different wavelengths probe different levels in the atmosphere, these variations track a wavelength-dependent set of radiative exchanges happening between different atmospheric levels as a perturbation evolves in time. We conclude that thermal-as well as cloud-fluctuations must be considered as possible contributors to the observed brown dwarf variability.
C1 [Robinson, Tyler D.; Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Robinson, Tyler D.] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA.
RP Robinson, TD (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.
EM tyler.d.robinson@nasa.gov
RI Marley, Mark/I-4704-2013;
OI Marley, Mark/0000-0002-5251-2943; Robinson, Tyler/0000-0002-3196-414X
FU NASA Astrobiology Institute's Virtual Planetary Laboratory
[NNH05ZDA001C]; NASA Planetary Atmospheres and Origins programs
FX T.R. gratefully acknowledges support from an appointment to the NASA
Postdoctoral Program at NASA Ames Research Center, administered by Oak
Ridge Affiliated Universities, and from the NASA Astrobiology
Institute's Virtual Planetary Laboratory, under solicitation No.
NNH05ZDA001C. M. M. acknowledges support of the NASA Planetary
Atmospheres and Origins programs. We thank Jonathan Fortney for sharing
tools for computing normalized contribution functions, Jacqueline
Radigan for reviewing an early version of this paper, and Caroline
Morley for sharing updates to relevant cloud routines in our thermal
structure model.
NR 35
TC 16
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2014
VL 785
IS 2
AR 158
DI 10.1088/0004-637X/785/2/158
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG9KA
UT WOS:000335736800077
ER
PT J
AU Spilker, JS
Marrone, DP
Aguirre, E
Aravena, M
Ashby, MLN
Bethermin, M
Bradford, CM
Bothwell, MS
Brodwin, M
Carlstrom, JE
Chapman, SC
Crawford, TM
de Breuck, C
Fassnacht, CD
Gonzalez, AH
Greve, TR
Gullberg, B
Hezaveh, Y
Holzapfel, WL
Husband, K
Ma, J
Malkan, M
Murphy, EJ
Reichardt, CL
Rotermund, KM
Stalder, B
Stark, AA
Strandet, M
Vieira, JD
Weiss, A
Welikala, N
AF Spilker, J. S
Marrone, D. P.
Aguirre, E.
Aravena, M.
Ashby, M. L. N.
Bethermin, M.
Bradford, C. M.
Bothwell, M. S.
Brodwin, M.
Carlstrom, J. E.
Chapman, S. C.
Crawford, T. M.
de Breuck, C.
Fassnacht, C. D.
Gonzalez, A. H.
Greve, T. R.
Gullberg, B.
Hezaveh, Y.
Holzapfel, W. L.
Husband, K.
Ma, J.
Malkan, M.
Murphy, E. J.
Reichardt, C. L.
Rotermund, K. M.
Stalder, B.
Stark, A. A.
Strandet, M.
Vieira, J. D.
Weiss, A.
Welikala, N.
TI THE REST-FRAME SUBMILLIMETER SPECTRUM OF HIGH-REDSHIFT, DUSTY,
STAR-FORMING GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: high-redshift; galaxies: ISM; galaxies: star formation; ISM:
molecules
ID DENSE MOLECULAR GAS; SOUTH-POLE TELESCOPE; ULTRALUMINOUS INFRARED
GALAXIES; DIFFUSE INTERSTELLAR-MEDIUM; CLOVERLEAF QUASAR; APM
08279+5255; CONVERSION FACTOR; HERSCHEL-SPIRE; LINE EMISSION; ARP 220
AB We present the average rest-frame spectrum of high-redshift dusty, star-forming galaxies from 250 to 770 GHz. This spectrum was constructed by stacking Atacama Large Millimeter/submillimeter Array (ALMA) 3 mm spectra of 22 such sources discovered by the South Pole Telescope and spanning z = 2.0-5.7. In addition to multiple bright spectral features of (CO)-C-12, [C I], and H2O, we also detect several faint transitions of (CO)-C-13, HCN, HNC, HCO+, and CN, and use the observed line strengths to characterize the typical properties of the interstellar medium of these high-redshift starburst galaxies. We find that the (CO)-C-13 brightness in these objects is comparable to that of the only otherz > 2 star-forming galaxy in which (CO)-C-13 has been observed. We show that the emission from the high-critical density molecules HCN, HNC, HCO+, and CN is consistent with a warm, dense medium with T-kin similar to 55K and n(H2) >= 10(5.5) cm(-3). High molecular hydrogen densities are required to reproduce the observed line ratios, and we demonstrate that alternatives to purely collisional excitation are unlikely to be significant for the bulk of these systems. We quantify the average emission from several species with no individually detected transitions, and find emission from the hydride CH and the linear molecule CCH for the first time at high redshift, indicating that these molecules may be powerful probes of interstellar chemistry in high-redshift systems. These observations represent the first constraints on many molecular species with rest-frame transitions from 0.4 to 1.2 mm in star-forming systems at high redshift, and will be invaluable in making effective use of ALMA in full science operations.
C1 [Spilker, J. S; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Aguirre, E.] Univ Penn, Philadelphia, PA 19104 USA.
[Aravena, M.] European So Observ, Casilla 19001, Vitacura Santia, Chile.
[Aravena, M.] Univ Diego Port, Fac Ingn, Santiago, Chile.
[Ashby, M. L. N.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bethermin, M.] Univ Paris Diderot, CEA Saclay, CEA DSM Irfu CNRS, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France.
[Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bothwell, M. S.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HA, England.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Carlstrom, J. E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Carlstrom, J. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Crawford, T. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Chapman, S. C.; Rotermund, K. M.] Dalhousie Univ, Halifax, NS, Canada.
[de Breuck, C.; Gullberg, B.] European So Observ, D-85748 Garching, Germany.
[Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Gonzalez, A. H.; Husband, K.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Hezaveh, Y.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Holzapfel, W. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Husband, K.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Malkan, M.] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Murphy, E. J.] Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Strandet, M.; Weiss, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Welikala, N.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France.
RP Spilker, JS (reprint author), Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
EM jspilker@as.arizona.edu
RI Aravena, Manuel/O-2361-2014; Holzapfel, William/I-4836-2015;
OI Bethermin, Matthieu/0000-0002-3915-2015; Stark,
Antony/0000-0002-2718-9996; Marrone, Daniel/0000-0002-2367-1080;
Reichardt, Christian/0000-0003-2226-9169; De Breuck,
Carlos/0000-0002-6637-3315
FU U.S. National Science Foundation [AST-1312950]; National Science
Foundation [ANT-0638937]; Kavli Foundation; Gordon and Betty Moore
Foundation; Commonwealth of Australia; [PHY-1125897]
FX This material is based on work supported by the U.S. National Science
Foundation under grant No. AST-1312950. The SPT is supported by the
National Science Foundation through grant ANT-0638937, with partial
support through PHY-1125897, the Kavli Foundation and the Gordon and
Betty Moore Foundation. This paper makes use of the following ALMA data:
ADS/JAO.ALMA2011.0.00957.S and 2011.0.00958.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. The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. The Australia Telescope
Compact Array is part of the Australia Telescope National Facility which
is funded by the Commonwealth of Australia for operation as a National
Facility managed by CSIRO. This research has made use of NASA's
Astrophysics Data System.
NR 119
TC 18
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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 APR 20
PY 2014
VL 785
IS 2
AR 149
DI 10.1088/0004-637X/785/2/149
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG9KA
UT WOS:000335736800068
ER
PT J
AU Bulyshev, A
Amzajerdian, F
Roback, VE
Hines, G
Pierrottet, D
Reisse, R
AF Bulyshev, Alexander
Amzajerdian, Farzin
Roback, Vincent E.
Hines, Glenn
Pierrottet, Diego
Reisse, Robert
TI Three-dimensional super-resolution: theory, modeling, and field test
results
SO APPLIED OPTICS
LA English
DT Article
ID IMAGE-RECONSTRUCTION
AB Many flash lidar applications continue to demand higher three-dimensional image resolution beyond the current state-of-the-art technology of the detector arrays and their associated readout circuits. Even with the available number of focal plane pixels, the required number of photons for illuminating all the pixels may impose impractical requirements on the laser pulse energy or the receiver aperture size. Therefore, image resolution enhancement by means of a super-resolution algorithm in near real time presents a very attractive solution for a wide range of flash lidar applications. This paper describes a super-resolution technique and illustrates its performance and merits for generating three-dimensional image frames at a video rate. (C) 2014 Optical Society of America
C1 [Bulyshev, Alexander] Analyt Mech Associates, Hampton, VA 23666 USA.
[Amzajerdian, Farzin; Roback, Vincent E.; Hines, Glenn; Reisse, Robert] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Pierrottet, Diego] Coherent Applicat Inc, Hampton, VA 23666 USA.
RP Bulyshev, A (reprint author), Analyt Mech Associates, Hampton, VA 23666 USA.
EM alexander.bulyshev-1@nasa.gov
NR 19
TC 6
Z9 6
U1 0
U2 19
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD APR 20
PY 2014
VL 53
IS 12
BP 2583
EP 2594
DI 10.1364/AO.53.002583
PG 12
WC Optics
SC Optics
GA AF2ZZ
UT WOS:000334582400005
PM 24787583
ER
PT J
AU Epstein, CR
Elsworth, YP
Johnson, JA
Shetrone, M
Mosser, B
Hekker, S
Tayar, J
Harding, P
Pinsonneault, M
Aguirre, VS
Basu, S
Beers, TC
Bizyaev, D
Bedding, TR
Chaplin, WJ
Frinchaboy, PM
Garcia, RA
Perez, AEG
Hearty, FR
Huber, D
Ivans, II
Majewski, SR
Mathur, S
Nidever, D
Serenelli, A
Schiavon, RP
Schneider, DP
Schonrichi, R
Sobeck, JS
Stassun, KG
Stello, D
Zasowski, G
AF Epstein, Courtney R.
Elsworth, Yvonne P.
Johnson, Jennifer A.
Shetrone, Matthew
Mosser, Benoit
Hekker, Saskia
Tayar, Jamie
Harding, Paul
Pinsonneault, Marc
Aguirre, Victor Silva
Basu, Sarbani
Beers, Timothy C.
Bizyaev, Dmitry
Bedding, Timothy R.
Chaplin, William J.
Frinchaboy, Peter M.
Garcia, Rafael A.
Perez, Ana E. Garcia
Hearty, Fred R.
Huber, Daniel
Ivans, Inese I.
Majewski, Steven R.
Mathur, Savita
Nidever, David
Serenelli, Aldo
Schiavon, Ricardo P.
Schneider, Donald P.
Schoenrichi, Ralph
Sobeck, Jennifer S.
Stassun, Keivan G.
Stello, Dennis
Zasowski, Gail
TI TESTING THE ASTEROSEISMIC MASS SCALE USING METAL-POOR STARS
CHARACTERIZED WITH APOGEE AND KEPLER
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE asteroseismology; Galaxy: halo; stars: fundamental parameters
ID SOLAR-LIKE OSCILLATIONS; DIGITAL SKY SURVEY; MILKY-WAY; NGC 6791;
GLOBULAR-CLUSTERS; RED GIANTS; HIPPARCOS PARALLAXES; STELLAR
POPULATIONS; BRANCH STARS; AGE
AB Fundamental stellar properties, such as mass, radius, and age, can be inferred using asteroseismology. Cool stars with convective envelopes have turbulent motions that can stochastically drive and damp pulsations. The properties of the oscillation frequency power spectrum can be tied to mass and radius through solar-scaled asteroseismic relations. Stellar properties derived using these scaling relations need verification over a range of metallicities. Because the age and mass of halo stars are well-constrained by astrophysical priors, they provide an independent, empirical check on asteroseismic mass estimates in the low-metallicity regime. We identify nine metal-poor red giants (including six stars that are kinematically associated with the halo) from a sample observed by both the Kepler space telescope and the Sloan Digital Sky Survey-III APOGEE spectroscopic survey. We compare masses inferred using asteroseismology to those expected for halo and thick-disk stars. Although our sample is small, standard scaling relations, combined with asteroseismic parameters from the APOKASC Catalog, produce masses that are systematically higher ((Delta M) = 0.17 +/- 0.05 M-circle dot) than astrophysical expectations. The magnitude of the mass discrepancy is reduced by known theoretical corrections to the measured large frequency separation scaling relationship. Using alternative methods for measuring asteroseismic parameters induces systematic shifts at the 0.04 M-circle dot level. We also compare published asteroseismic analyses with scaling relationship masses to examine the impact of using the frequency of maximum power as a constraint. Upcoming APOKASC observations will provide a larger sample of similar to 100 metal-poor stars, important for detailed asteroseismic characterization of Galactic stellar populations.
C1 [Epstein, Courtney R.; Johnson, Jennifer A.; Tayar, Jamie; Pinsonneault, Marc; Schoenrichi, Ralph; Zasowski, Gail] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Elsworth, Yvonne P.; Chaplin, William J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Johnson, Jennifer A.; Zasowski, Gail] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Shetrone, Matthew] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Mosser, Benoit] Univ Paris 06, Univ Denis Diderot, Observ Paris, LESIA,CNRS, F-92195 Meudon, France.
[Hekker, Saskia] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
[Harding, Paul] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA.
[Aguirre, Victor Silva] Dept Phys & Astron, Stellar Astrophys Ctr, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Beers, Timothy C.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Beers, Timothy C.] JINA, Sunspot, NM 88349 USA.
[Bizyaev, Dmitry] Apache Point Observ, Sunspot, NM 88349 USA.
[Bedding, Timothy R.; Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Frinchaboy, Peter M.] Texas Christian Univ, Dept Phys & Astron, Ft Worth, TX 76129 USA.
[Garcia, Rafael A.] Univ Paris 07, CEA DSM CNRS, Ctr Saclay, IRFU SAp,Lab AIM, F-91191 Gif Sur Yvette, France.
[Perez, Ana E. Garcia; Hearty, Fred R.; Majewski, Steven R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ivans, Inese I.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Mathur, Savita] Space Sci Inst, Boulder, CO 80301 USA.
[Nidever, David] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Serenelli, Aldo] IEEC CSIC, Inst Space Sci, Fac Cincies, Campus UAB, E-08193 Bellaterra, Spain.
[Schiavon, Ricardo P.] Liverpool John Moores Univ, IC2, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Schoenrichi, Ralph] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England.
[Sobeck, Jennifer S.] Univ Chicago, JINA, Chicago, IL 60637 USA.
[Sobeck, Jennifer S.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Zasowski, Gail] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Epstein, CR (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
EM epstein@astronomy.ohio-state.edu
OI Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661;
Garcia, Rafael/0000-0002-8854-3776; Serenelli, Aldo/0000-0001-6359-2769
FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department
of Energy Office of Science; University of Arizona; Brazilian
Participation Group; Brookhaven National Laboratory; Carnegie Mellon
University; University of Florida; French Participation Group; German
Participation Group; Harvard University; Instituto de Astrofisica de
Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns
Hopkins University; Lawrence Berkeley National Laboratory; Max Planck
Institute for Astrophysics; Max Planck Institute for Extraterrestrial
Physics; New Mexico State University; New York University; Ohio State
University; Pennsylvania State University; University of Portsmouth;
Princeton University; Spanish Participation Group; University of Tokyo;
University of Utah; Vanderbilt University; University of Virginia;
University of Washington; Yale University; Physics Frontier Center/Joint
Institute for Nuclear Astrophysics (JINA) [PHY 08-22648]; NASA
[NNX12AE17G]; Netherlands Organization for Scientific Research; ERC
[338251]; MICINN [AYA2011-24704]; Danish National Research Foundation
[DNRF106]; ASTERISK project (AS-TERoseismic Investigations with SONG and
Kepler); European Research Council [267864]; [AST-1211673]
FX Funding for SDSS-III has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, and the U.S. Department of Energy Office of Science. The
SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the
Astrophysical Research Consortium for the Participating Institutions of
the SDSS-III Collaboration including the University of Arizona, the
Brazilian Participation Group, Brookhaven National Laboratory, Carnegie
Mellon University, University of Florida, the French Participation
Group, the German Participation Group, Harvard University, the Instituto
de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA
Participation Group, Johns Hopkins University, Lawrence Berkeley
National Laboratory, Max Planck Institute for Astrophysics, Max Planck
Institute for Extraterrestrial Physics, New Mexico State University, New
York University, Ohio State University, Pennsylvania State University,
University of Portsmouth, Princeton University, the Spanish
Participation Group, University of Tokyo, University of Utah, Vanderbilt
University, University of Virginia, University of Washington, and Yale
University.; We thank Andrea Miglio and the APOKASC team for helpful
discussions. C. R. E., J.A.J., and M. P. acknowledge support by
AST-1211673, T. C. B. by PHY 08-22648: Physics Frontier Center/Joint
Institute for Nuclear Astrophysics (JINA), and S. M. by the NASA grant
NNX12AE17G. S. H. acknowledges support from the Netherlands Organization
for Scientific Research and ERC Starting Grant #338251 Stellar Ages. A.
S. is partially supported by the MICINN grant AYA2011-24704. Funding for
the Stellar Astrophysics Centre is provided by The Danish National
Research Foundation (grant agreement No. DNRF106). V. S. A. is supported
by the ASTERISK project (AS-TERoseismic Investigations with SONG and
Kepler) funded by the European Research Council (grant agreement No.
267864).
NR 50
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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 APR 20
PY 2014
VL 785
IS 2
AR L28
DI 10.1088/2041-8205/785/2/L28
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE9VR
UT WOS:000334359800009
ER
PT J
AU Kipping, DM
Bastien, FA
Stassun, KG
Chaplin, WJ
Huber, D
Buchhave, LA
AF Kipping, D. M.
Bastien, F. A.
Stassun, K. G.
Chaplin, W. J.
Huber, D.
Buchhave, L. A.
TI FLICKER AS A TOOL FOR CHARACTERIZING PLANETS THROUGH ASTERODENSITY
PROFILING
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planetary systems; stars: activity; stars: solar-type; techniques:
photometric
ID CANDIDATE HOST STARS; FIELD STARS; ASTEROSEISMOLOGY; OSCILLATIONS;
ROTATION; AGES; VARIABILITY
AB Variability in the time series brightness of a star on a timescale of 8 hr, known as "flicker," has been previously demonstrated to serve as a proxy for the surface gravity of a star by Bastien et al. Although surface gravity is crucial for stellar classification, it is the mean stellar density that is most useful when studying transiting exoplanets, due to its direct impact on the transit light curve shape. Indeed, an accurate and independent measure of the stellar density can be leveraged to infer subtle properties of a transiting system, such as the companion's orbital eccentricity via asterodensity profiling (AP). We here calibrate flicker to the mean stellar density of 439 Kepler targets with asteroseismology, allowing us to derive a new empirical relation given by log(10)(rho star (kg m(- 3))) = 5.413 - 1.850 log(10)(F-8 (ppm)). The calibration is valid for stars with 4500 < T-eff < 6500 K, KP < 14, and flicker estimates corresponding to stars with 3.25 < log g star < 4.43. Our relation has a model error in the stellar density of 31.7% and so has similar to 8 times lower precision than that from asteroseismology but is applicable to a sample similar to 40 times greater. Flicker therefore provides an empirical method to enable AP on hundreds of planetary candidates from present and future missions.
C1 [Kipping, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bastien, F. A.; Stassun, K. G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Stassun, K. G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
[Chaplin, W. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Chaplin, W. J.] Aarhus Univ, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huber, D.] SETI Inst, Mountain View, CA 94043 USA.
[Buchhave, L. A.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dkipping@cfa.harvard.edu
OI Buchhave, Lars A./0000-0003-1605-5666; Stassun,
Keivan/0000-0002-3481-9052
FU NASA Sagan Fellowship; NASA Harriet Jenkins Fellowship; Vanderbilt
Provost Graduate Fellowship; UK Science and Technology Facilities
Council; NASA Postdoctoral Program at Ames Research Center; Kepler
Participating Scientist Program
FX D.M.K. is supported by the NASA Sagan Fellowships. F. A. B. is supported
by the NASA Harriet Jenkins Fellowship and a Vanderbilt Provost Graduate
Fellowship. W.J.C. acknowledges financial support from the UK Science
and Technology Facilities Council. D. H. acknowledges support by an
appointment to the NASA Postdoctoral Program at Ames Research Center,
administered by Oak Ridge Associated Universities through a contract
with NASA, and support by the Kepler Participating Scientist Program. We
thank the anaon.
NR 33
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 20
PY 2014
VL 785
IS 2
AR L32
DI 10.1088/2041-8205/785/2/L32
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE9VR
UT WOS:000334359800013
ER
PT J
AU Yamaguchi, H
Badenes, C
Petre, R
Nakano, T
Castro, D
Enoto, T
Hiraga, JS
Hughes, JP
Maeda, Y
Nobukawa, M
Safi-Harb, S
Slane, PO
Smith, RK
Uchida, H
AF Yamaguchi, Hiroya
Badenes, Carles
Petre, Robert
Nakano, Toshio
Castro, Daniel
Enoto, Teruaki
Hiraga, Junko S.
Hughes, John P.
Maeda, Yoshitomo
Nobukawa, Masayoshi
Safi-Harb, Samar
Slane, Patrick O.
Smith, Randall K.
Uchida, Hiroyuki
TI DISCRIMINATING THE PROGENITOR TYPE OF SUPERNOVA REMNANTS WITH IRON
K-SHELL EMISSION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: abundances; ISM: supernova remnants; X-rays: ISM
ID X-RAY-EMISSION; LARGE-MAGELLANIC-CLOUD; XMM-NEWTON OBSERVATIONS; IA
SUPERNOVA; SHOCKED EJECTA; RCW 86; CHANDRA; SPECTROSCOPY; EXPLOSION;
SUZAKU
AB Supernova remnants (SNRs) retain crucial information about both their parent explosion and circumstellar material left behind by their progenitor. However, the complexity of the interaction between supernova ejecta and ambient medium often blurs this information, and it is not uncommon for the basic progenitor type (Ia or core-collapse) of well-studied remnants to remain uncertain. Here we present a powerful new observational diagnostic to discriminate between progenitor types and constrain the ambient medium density of SNRs using solely Fe K-shell X-ray emission. We analyze all extant Suzaku observations of SNRs and detect Fe K alpha emission from 23 young or middle-aged remnants, including five first detections (IC 443, G292.0+ 1.8, G337.2-0.7, N49, and N63A). The Fe Ka centroids clearly separate progenitor types, with the Fe-rich ejecta in Type Ia remnants being significantly less ionized than in core-collapse SNRs. Within each progenitor group, the Fe Ka luminosity and centroid are well correlated, with more luminous objects having more highly ionized Fe. Our results indicate that there is a strong connection between explosion type and ambient medium density, and suggest that Type Ia supernova progenitors do not substantially modify their surroundings at radii of up to several parsecs. We also detect a K-shell radiative recombination continuum of Fe in W49B and IC 443, implying a strong circumstellar interaction in the early evolutionary phases of these core-collapse remnants.
C1 [Yamaguchi, Hiroya; Petre, Robert; Enoto, Teruaki] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yamaguchi, Hiroya] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Yamaguchi, Hiroya; Slane, Patrick O.; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Badenes, Carles] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Badenes, Carles] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA.
[Badenes, Carles] Univ Pittsburgh, Pittsburgh, PA 15260 USA.
[Nakano, Toshio; Hiraga, Junko S.] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan.
[Castro, Daniel] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA.
[Enoto, Teruaki] RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan.
[Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Maeda, Yoshitomo] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Nobukawa, Masayoshi] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Safi-Harb, Samar] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada.
RP Yamaguchi, H (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
EM hiroya.yamaguchi@nasa.gov
RI XRAY, SUZAKU/A-1808-2009;
OI Enoto, Teruaki/0000-0003-1244-3100
NR 51
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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
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 20
PY 2014
VL 785
IS 2
AR L27
DI 10.1088/2041-8205/785/2/L27
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE9VR
UT WOS:000334359800008
ER
PT J
AU Sidery, T
Aylott, B
Christensen, N
Farr, B
Farr, W
Feroz, F
Gair, J
Grover, K
Graff, P
Hanna, C
Kalogera, V
Mandel, I
O'Shaughnessy, R
Pitkin, M
Price, L
Raymond, V
Rover, C
Singer, L
van der Sluys, M
Smith, RJE
Vecchio, A
Veitch, J
Vitale, S
AF Sidery, T.
Aylott, B.
Christensen, N.
Farr, B.
Farr, W.
Feroz, F.
Gair, J.
Grover, K.
Graff, P.
Hanna, C.
Kalogera, V.
Mandel, I.
O'Shaughnessy, R.
Pitkin, M.
Price, L.
Raymond, V.
Roever, C.
Singer, L.
van der Sluys, M.
Smith, R. J. E.
Vecchio, A.
Veitch, J.
Vitale, S.
TI Reconstructing the sky location of gravitational-wave detected compact
binary systems: Methodology for testing and comparison
SO PHYSICAL REVIEW D
LA English
DT Article
ID ELECTROMAGNETIC COUNTERPARTS; INSPIRALS
AB The problem of reconstructing the sky position of compact binary coalescences detected via gravitational waves is a central one for future observations with the ground-based network of gravitational-wave laser interferometers, such as Advanced LIGO and Advanced Virgo. Different techniques for sky localization have been independently developed. They can be divided in two broad categories: fully coherent Bayesian techniques, which are high latency and aimed at in-depth studies of all the parameters of a source, including sky position, and "triangulation-based" techniques, which exploit the data products from the search stage of the analysis to provide an almost real-time approximation of the posterior probability density function of the sky location of a detection candidate. These techniques have previously been applied to data collected during the last science runs of gravitational-wave detectors operating in the so-called initial configuration. Here, we develop and analyze methods for assessing the self consistency of parameter estimation methods and carrying out fair comparisons between different algorithms, addressing issues of efficiency and optimality. These methods are general, and can be applied to parameter estimation problems other than sky localization. We apply these methods to two existing sky localization techniques representing the two above-mentioned categories, using a set of simulated inspiral-only signals from compact binary systems with a total mass of <= 20M(circle dot) and nonspinning components. We compare the relative advantages and costs of the two techniques and show that sky location uncertainties are on average a factor approximate to 20 smaller for fully coherent techniques than for the specific variant of the triangulation-based technique used during the last science runs, at the expense of a factor approximate to 1000 longer processing time.
C1 [Sidery, T.; Farr, B.; Farr, W.; Grover, K.; Mandel, I.; Smith, R. J. E.; Vecchio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Christensen, N.] Carleton Coll, Northfield, MN 55057 USA.
[Farr, B.; Farr, W.; Kalogera, V.] Northwestern Univ, Dept Phys & Astron, CIERA, Evanston, IL 60208 USA.
[Feroz, F.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England.
[Gair, J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Graff, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hanna, C.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[O'Shaughnessy, R.] Univ Wisconsin, Ctr Gravitat & Cosmol, Milwaukee, WI 53211 USA.
[Pitkin, M.] Univ Glasgow, SUPA, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Price, L.; Raymond, V.; Singer, L.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Roever, C.] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-30167 Hannover, Germany.
[Roever, C.] Univ Med Ctr, Dept Med Stat, D-37073 Gottingen, Germany.
[van der Sluys, M.] Radboud Univ Nijmegen, NL-6500 GL Nijmegen, Netherlands.
[Veitch, J.] Nikhef, NL-1098 XG Amsterdam, Netherlands.
[Vitale, S.] MIT, Cambridge, MA 02139 USA.
RP Sidery, T (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
EM tsidery@star.sr.bham.ac.uk
RI Vecchio, Alberto/F-8310-2015;
OI Vecchio, Alberto/0000-0002-6254-1617; Rover,
Christian/0000-0002-6911-698X; Farr, Ben/0000-0002-2916-9200;
O'Shaughnessy, Richard/0000-0001-5832-8517; Mandel,
Ilya/0000-0002-6134-8946; Pitkin, Matthew/0000-0003-4548-526X; Veitch,
John/0000-0002-6508-0713
FU Foundation for Fundamental Research on Matter (FOM); Netherlands
Organization for Scientific Research (NWO); NSF [PHY-1204371,
PHY-1307020, DGE-0824162, PHY-0970074, PHY-0757058]; Oak Ridge
Associated Universities; California Institute of Technology division of
Physics, Mathematics Astronomy; LIGO Laboratory; UWM Research Growth
Initiative
FX J.V. was supported by the research program of the Foundation for
Fundamental Research on Matter (FOM), which is partially supported by
the Netherlands Organization for Scientific Research (NWO). N.C. was
supported by the NSF Grant No. PHY-1204371. P.G. was supported by a NASA
postdoctoral fellowship from the Oak Ridge Associated Universities.
B.F., W.F. and V.K. were supported by the NSF Grant No. PHY-1307020, and
B.F. was also supported by the NSF Grant No. DGE-0824162. V.R. was
supported by a prize postdoctoral fellowship from the California
Institute of Technology division of Physics, Mathematics & Astronomy and
LIGO Laboratory. R.O.S. was supported by the NSF Grant No. PHY-0970074
and the UWM Research Growth Initiative. S.V. acknowledges 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 no. PHY-0757058.
NR 39
TC 25
Z9 25
U1 0
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD APR 18
PY 2014
VL 89
IS 8
AR 084060
DI 10.1103/PhysRevD.89.084060
PG 11
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AG2HH
UT WOS:000335236500004
ER
PT J
AU Schmidt, GA
AF Schmidt, Gavin A.
TI Behind the Curve Science and the Politics of Global Warming
SO SCIENCE
LA English
DT Book Review
C1 [Schmidt, Gavin A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Schmidt, GA (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM gs210@columbia.edu
RI Schmidt, Gavin/D-4427-2012
OI Schmidt, Gavin/0000-0002-2258-0486
NR 2
TC 0
Z9 0
U1 1
U2 11
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD APR 18
PY 2014
VL 344
IS 6181
BP 256
EP 256
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AF1LD
UT WOS:000334474500019
ER
PT J
AU Quintana, EV
Barclay, T
Raymond, SN
Rowe, JF
Bolmont, E
Caldwell, DA
Howell, SB
Kane, SR
Huber, D
Crepp, JR
Lissauer, JJ
Ciardi, DR
Coughlin, JL
Everett, ME
Henze, CE
Horch, E
Isaacson, H
Ford, EB
Adams, FC
Still, M
Hunter, RC
Quarles, B
Selsis, F
AF Quintana, Elisa V.
Barclay, Thomas
Raymond, Sean N.
Rowe, Jason F.
Bolmont, Emeline
Caldwell, Douglas A.
Howell, Steve B.
Kane, Stephen R.
Huber, Daniel
Crepp, Justin R.
Lissauer, Jack J.
Ciardi, David R.
Coughlin, Jeffrey L.
Everett, Mark E.
Henze, Christopher E.
Horch, Elliott
Isaacson, Howard
Ford, Eric B.
Adams, Fred C.
Still, Martin
Hunter, Roger C.
Quarles, Billy
Selsis, Franck
TI An Earth-Sized Planet in the Habitable Zone of a Cool Star
SO SCIENCE
LA English
DT Article
ID LOW-MASS STARS; MAIN-SEQUENCE STARS; M-DWARF STARS; SUN-LIKE STAR;
SUPER-EARTHS; ECLIPSING BINARY; GLIESE 581D; SYSTEMS; VALIDATION; RADII
AB The quest for Earth-like planets is a major focus of current exoplanet research. Although planets that are Earth-sized and smaller have been detected, these planets reside in orbits that are too close to their host star to allow liquid water on their surfaces. We present the detection of Kepler-186f, a 1.11 +/- 0.14 Earth-radius planet that is the outermost of five planets, all roughly Earth-sized, that transit a 0.47 +/- 0.05 solar-radius star. The intensity and spectrum of the star's radiation place Kepler-186f in the stellar habitable zone, implying that if Kepler-186f has an Earth-like atmosphere and water at its surface, then some of this water is likely to be in liquid form.
C1 [Quintana, Elisa V.; Rowe, Jason F.; Caldwell, Douglas A.; Huber, Daniel; Coughlin, Jeffrey L.] SETI Inst, Mountain View, CA 94043 USA.
[Quintana, Elisa V.; Barclay, Thomas; Rowe, Jason F.; Caldwell, Douglas A.; Howell, Steve B.; Huber, Daniel; Lissauer, Jack J.; Coughlin, Jeffrey L.; Henze, Christopher E.; Hunter, Roger C.; Quarles, Billy] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, West Sonoma, CA 95476 USA.
[Raymond, Sean N.; Bolmont, Emeline; Selsis, Franck] Univ Bordeaux, Lab Astrophys Bordeaux, UMR 5804, F-33270 Floirac, France.
[Raymond, Sean N.; Bolmont, Emeline; Selsis, Franck] CNRS, Lab Astrophys Bordeaux, UMR 5804, F-33270 Floirac, France.
[Kane, Stephen R.] San Francisco State Univ, San Francisco, CA 94132 USA.
[Crepp, Justin R.] Univ Notre Dame, Notre Dame, IN 46556 USA.
[Lissauer, Jack J.] Stanford Univ, Dept Geol & Environm Sci, Stanford, CA 94305 USA.
[Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Horch, Elliott] So Connecticut State Univ, New Haven, CT 06515 USA.
[Isaacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Ford, Eric B.] Penn State Univ, Davey Lab 525, Ctr Exoplanets & Habitable, University Pk, PA 16802 USA.
[Ford, Eric B.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Adams, Fred C.] Univ Michigan, Dept Phys, Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA.
[Adams, Fred C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
RP Quintana, EV (reprint author), SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA.
EM elisa.quintana@nasa.gov
RI Caldwell, Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; Ciardi, David/0000-0002-5741-3047
FU Research Opportunities in Space and Earth Sciences Kepler Participating
Scientist Program [NNX12AD21G]; NASA [NNA13AA93A, NAS5-26555]; NASA
Postdoctoral Program at the Ames Research Center; Kepler Participating
Scientist Program; Pennsylvania State University; Eberly College of
Science; Pennsylvania Space Grant Consortium; European Research Council
[209622: E3ARTHs]; NASA Science Mission directorate; NASA Office of
Space Science [NNX13AC07G]; National Science Foundation (NSF); National
Research Council (Canada); Comision Nacional de Investigacion Cientifica
y Tecnologica (Chile); Australian Research Council (Australia);
Ministerio da Ciencia, Tecnologia e Inovacao (Brazil); Ministerio de
Ciencia, Tecnologia e Innovacion Productiva (Argentina)
FX The authors working at NASA Ames thank the SETI Institute for hosting
them during the U. S. government shutdown. E. V. Q. and J.F.R.
acknowledge support from the Research Opportunities in Space and Earth
Sciences Kepler Participating Scientist Program Grant NNX12AD21G.
S.N.R.'s contribution was performed as part of the NASA Astrobiology
Institute's Virtual Planetary Laboratory Lead Team, supported by NASA
under cooperative agreement no. NNA13AA93A. D. H. acknowledges support
by an appointment to the NASA Postdoctoral Program at the Ames Research
Center, administered by Oak Ridge Associated Universities through a
contract with NASA, and the Kepler Participating Scientist Program. The
Center for Exoplanets and Habitable Worlds is supported by the
Pennsylvania State University, the Eberly College of Science, and the
Pennsylvania Space Grant Consortium. F. S. acknowledges support from the
European Research Council (Starting Grant 209622: E3ARTHs). This paper
includes data collected by the Kepler mission. Funding for the Kepler
mission is provided by the NASA Science Mission directorate. This
research also made use of NASA's Astrophysics Data System. Some of the
data presented in this paper were obtained from the Mikulski Archive for
Space Telescopes (MAST). The Space Telescope Science Institute is
operated by the Association of Universities for Research in Astronomy,
under NASA contract NAS5-26555. Support for MAST for non-Hubble Space
Telescope data is provided by the NASA Office of Space Science via grant
NNX13AC07G and by other grants and contracts. This research made use of
the NASA Exoplanet Archive, which is operated by the California
Institute of Technology, under contract with NASA under the Exoplanet
Exploration Program. The Gemini Observatory is operated by the
Association of Universities for Research in Astronomy, under a
cooperative agreement with the National Science Foundation (NSF) on
behalf of the Gemini partnership: NSF (United States), the National
Research Council (Canada), the Comision Nacional de Investigacion
Cientifica y Tecnologica (Chile), the Australian Research Council
(Australia), the Ministerio da Ciencia, Tecnologia e Inovacao (Brazil),
and the Ministerio de Ciencia, Tecnologia e Innovacion Productiva
(Argentina).
NR 37
TC 88
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U1 28
U2 136
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD APR 18
PY 2014
VL 344
IS 6181
BP 277
EP 280
DI 10.1126/science.1249403
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AF1LD
UT WOS:000334474500029
PM 24744370
ER
PT J
AU Barcelo, SJ
Kim, A
Gibson, GA
Norris, KJ
Yamakawa, M
Li, ZY
AF Barcelo, Steven J.
Kim, Ansoon
Gibson, Gary A.
Norris, Kate J.
Yamakawa, Mineo
Li, Zhiyong
TI Deterministic nanoparticle assemblies: from substrate to solution
SO NANOTECHNOLOGY
LA English
DT Article
DE nanoparticle; self-assembly; plasmonics; SERS; chemical sensing
ID ENHANCED RAMAN-SCATTERING; LIVING MICE; GOLD; SURFACE; SPECTROSCOPY;
NANOSTRUCTURES; ARRAYS; SILVER; JUNCTIONS; TRIMERS
AB The deterministic assembly of metallic nanoparticles is an exciting field with many potential benefits. Many promising techniques have been developed, but challenges remain, particularly for the assembly of larger nanoparticles which often have more interesting plasmonic properties. Here we present a scalable process combining the strengths of top down and bottom up fabrication to generate deterministic 2D assemblies of metallic nanoparticles and demonstrate their stable transfer to solution. Scanning electron and high-resolution transmission electron microscopy studies of these assemblies suggested the formation of nanobridges between touching nanoparticles that hold them together so as to maintain the integrity of the assembly throughout the transfer process. The application of these nanoparticle assemblies as solution-based surface-enhanced Raman scattering (SERS) materials is demonstrated by trapping analyte molecules in the nanoparticle gaps during assembly, yielding uniformly high enhancement factors at all stages of the fabrication process.
C1 [Barcelo, Steven J.; Gibson, Gary A.; Yamakawa, Mineo; Li, Zhiyong] Hewlett Packard Labs, Palo Alto, CA 94043 USA.
[Kim, Ansoon] Korea Res Inst Stand & Sci, Taejon, South Korea.
[Norris, Kate J.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.
[Norris, Kate J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Barcelo, SJ (reprint author), Hewlett Packard Labs, Palo Alto, CA 94043 USA.
EM Zhiyong.li@hp.com
NR 45
TC 2
Z9 2
U1 6
U2 57
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
EI 1361-6528
J9 NANOTECHNOLOGY
JI Nanotechnology
PD APR 18
PY 2014
VL 25
IS 15
AR 155302
DI 10.1088/0957-4484/25/15/155302
PG 6
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA AD6TN
UT WOS:000333394100006
PM 24642827
ER
PT J
AU Franz, HB
Kim, ST
Farquhar, J
Day, JMD
Economos, RC
McKeegan, KD
Schmitt, AK
Irving, AJ
Hoek, J
Dottin, J
AF Franz, Heather B.
Kim, Sang-Tae
Farquhar, James
Day, James M. D.
Economos, Rita C.
McKeegan, Kevin D.
Schmitt, Axel K.
Irving, Anthony J.
Hoek, Joost
Dottin, James, III
TI Isotopic links between atmospheric chemistry and the deep sulphur cycle
on Mars
SO NATURE
LA English
DT Article
ID MARTIAN METEORITE; MINERAL ASSEMBLAGES; LOS-ANGELES; PETROGENESIS;
NAKHLITES; CHONDRITES; COMPONENTS; REGOLITH; ALH84001; SULFATE
AB The geochemistry of Martian meteorites provides a wealth of information about the solid planet and the surface and atmospheric processes that occurred on Mars. The degree to which Martian magmas may have assimilated crustal material, thus altering the geochemical signatures acquired from their mantle sources, is unclear(1). This issue features prominently in efforts to understand whether the source of light rare-earth elements in enriched shergottites lies in crustal material incorporated into melts(1,2) or in mixing between enriched and depleted mantle reservoirs(3). Sulphur isotope systematics offer insight into some aspects of crustal assimilation. The presence of igneous sulphides in Martian meteorites with sulphur isotope signatures indicative of mass-independent fractionation suggests the assimilation of sulphur both during passage of magmas through the crust of Mars and at sites of emplacement. Here we report isotopic analyses of 40 Martian meteorites that represent more than half of the distinct known Martian meteorites, including 30 shergottites (28 plus 2 pairs, where pairs are separate fragments of a single meteorite), 8 nakhlites (5 plus 3 pairs), Allan Hills 84001 and Chassigny. Our data provide strong evidence that assimilation of sulphur into Martian magmas was a common occurrence throughout much of the planet's history. The signature of mass-independent fractionation observed also indicates that the atmospheric imprint of photochemical processing preserved in Martian meteoritic sulphide and sulphate is distinct from that observed in terrestrial analogues, suggesting fundamental differences between the dominant sulphur chemistry in the atmosphere of Mars and that in the atmosphere of Earth(4).
C1 [Franz, Heather B.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Franz, Heather B.; Farquhar, James; Hoek, Joost; Dottin, James, III] Univ Maryland, Dept Geol, College Pk, MD 20742 USA.
[Franz, Heather B.; Farquhar, James; Hoek, Joost; Dottin, James, III] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Kim, Sang-Tae] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON L8S 4K1, Canada.
[Day, James M. D.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Economos, Rita C.; McKeegan, Kevin D.; Schmitt, Axel K.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Irving, Anthony J.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
RP Franz, HB (reprint author), NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
EM heather.b.franz@nasa.gov
RI McKeegan, Kevin/A-4107-2008; Kim, Sang-Tae/C-2768-2013; UCLA,
SIMS/A-1459-2011;
OI McKeegan, Kevin/0000-0002-1827-729X; Schmitt, Axel/0000-0002-9029-4211
FU US National Science Foundation Instrumentation and Facilities Program;
NASA Cosmochemistry grants [NNX09AF72G, NNX13AL13G]
FX We acknowledge the Meteorite Working Group, L. Welzenbach, T. McCoy, S.
Ralew, M. N. Rao, L. Nyquist, J. Zipfel, C. Smith, H. Kojima, A.
Treiman, T. Bunch and B. Zanda for providing meteorite samples analysed
in this study. We also thank P. Piccoli for assistance with electron
microprobe analyses. The manuscript benefited from independent reviews
by M. Thiemens, P. Cartigny, S. Ono, D. Johnston and B. Wing during
revision. The UCLA ion microprobe facility is partly supported by a
grant from the US National Science Foundation Instrumentation and
Facilities Program. This work was supported by NASA Cosmochemistry
grants NNX09AF72G and NNX13AL13G to J.F.
NR 38
TC 25
Z9 25
U1 5
U2 62
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD APR 17
PY 2014
VL 508
IS 7496
BP 364
EP +
DI 10.1038/nature13175
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AF0KP
UT WOS:000334403000045
PM 24740066
ER
PT J
AU Ackermann, M
Ajello, M
Albert, A
Allafort, A
Baldini, L
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Blandford, RD
Bloom, ED
Bonamente, E
Bottacini, E
Bouvier, A
Brandt, TJ
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 Angelis, A
de Palma, F
Dermer, CD
Digel, SW
Di Venere, L
Silva, EDE
Drell, PS
Drlica-Wagner, A
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Franckowiak, A
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Gomez-Vargas, GA
Grenier, IA
Grove, JE
Guiriec, S
Gustafsson, M
Hadasch, D
Hanabata, Y
Harding, AK
Hayashida, M
Hayashi, K
Hewitt, JW
Horan, D
Hou, X
Hughes, RE
Inoue, Y
Jackson, MS
Jogler, T
Johannesson, G
Johnson, AS
Kamae, T
Kawano, T
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Latronico, L
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Mayer, M
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
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
Razzaque, S
Reimer, A
Reimer, O
Ritz, S
Roth, M
Schaal, M
Schulz, A
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Strong, AW
Takahashi, H
Takeuchi, Y
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Tronconi, V
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Werner, M
Winer, BL
Wood, KS
Wood, M
Yang, Z
AF Ackermann, M.
Ajello, M.
Albert, A.
Allafort, A.
Baldini, L.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Bottacini, E.
Bouvier, A.
Brandt, T. 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 Angelis, A.
de Palma, F.
Dermer, C. D.
Digel, S. W.
Di Venere, L.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Franckowiak, A.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Gomez-Vargas, G. A.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Gustafsson, M.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashida, M.
Hayashi, K.
Hewitt, J. W.
Horan, D.
Hou, X.
Hughes, R. E.
Inoue, Y.
Jackson, M. S.
Jogler, T.
Johannesson, G.
Johnson, A. S.
Kamae, T.
Kawano, T.
Knoedlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Latronico, L.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Mayer, M.
Mazziotta, M. N.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Moiseev, A. A.
Monte, C.
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.
Panetta, J. H.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Ritz, S.
Roth, M.
Schaal, M.
Schulz, A.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Strong, A. W.
Takahashi, H.
Takeuchi, Y.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Tronconi, V.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Werner, M.
Winer, B. L.
Wood, K. S.
Wood, M.
Yang, Z.
CA LAT Collaboration
TI Inferred Cosmic-Ray Spectrum from Fermi Large Area Telescope gamma-Ray
Observations of Earth's Limb
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID ENERGY-SPECTRUM; HELIUM SPECTRA; EMISSION; GALAXY; ATMOSPHERE; PROTON;
ALBEDO; MODEL; EGRET
AB Recent accurate measurements of cosmic-ray (CR) species by ATIC-2, CREAM, and PAMELA reveal an unexpected hardening in the proton and He spectra above a few hundred GeV, a gradual softening of the spectra just below a few hundred GeV, and a harder spectrum of He compared to that of protons. These newly discovered features may offer a clue to the origin of high-energy CRs. We use the Fermi Large Area Telescope observations of the gamma-ray emission from Earth's limb for an indirect measurement of the local spectrum of CR protons in the energy range similar to 90 GeV-6 TeV (derived from a photon energy range 15 GeV-1 TeV). Our analysis shows that single power law and broken power law spectra fit the data equally well and yield a proton spectrum with index 2.68 +/- 0.04 and 2.61 +/- 0.08 above similar to 200 GeV, respectively.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Albert, A.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Okumura, A.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, WW Hansen Expt Phys, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Albert, A.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Okumura, A.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento 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.; Tronconi, V.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, 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.
[Bouvier, A.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Bouvier, A.; Ritz, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Brandt, T. J.; Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hewitt, J. W.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Brigida, M.; de Palma, F.; Di Venere, L.; 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.] Consorzio Interuniv Fis Spaziale, I-10133 Turin, Italy.
[Caraveo, P. A.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France.
[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 ASI Sci Data Ctr, I-00044 Rome, Italy.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] Ist Nazl Astrofis Osservatorio Astron Roma, I-00040 Rome, Italy.
[Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univ & Particules Montpellier, CNRS, IN2P3, Montpellier, France.
[Conrad, J.; Larsson, S.] Univ Stockholm, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.; Jackson, M. S.; Larsson, S.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden.
[Conrad, J.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etudes Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Dalton, M.; Hou, X.; Mehault, J.] INAF, Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] Univ Udine, Dipartmento Fis, I-33100 Udine, Italy.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[de Angelis, A.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Dermer, C. D.; Drlica-Wagner, A.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Fukazawa, Y.; Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Gomez-Vargas, G. A.; Morselli, A.; Vitale, V.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
[Gomez-Vargas, G. A.] Univ Autonoma Madrid, Inst Fis Teor, IFT UAM CSIC, E-28049 Madrid, Spain.
[Gomez-Vargas, G. A.] Univ Libre Bruxelles, Serv Phys Theor, B-1050 Brussels, Belgium.
[Guiriec, S.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Guiriec, S.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Gustafsson, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan.
[Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] JAXA, Inst Space & Aeronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Hanabata, Y.; Hayashida, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA.
[Hayashi, K.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Hughes, R. E.; Winer, B. L.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Jackson, M. S.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Johannesson, G.] Univ Toulouse, GAHEC, UPS OMP, IRAP, F-31028 Toulouse, France.
[Knoedlseder, J.] Univ Stockholm, Dept Astron, SE-10691 Stockholm, Sweden.
[Knoedlseder, J.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Larsson, S.; McEnery, J. E.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Larsson, S.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Latronico, L.] Mahidol Univ, Fac Sci, Dept Phys, Bangkok 10400, Thailand.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Mitthumsiri, W.; Moiseev, A. A.] Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Mitthumsiri, W.; Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA.
[Moiseev, A. A.; Nemmen, R.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Moiseev, A. A.; Nemmen, R.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Murgia, S.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Nemmen, R.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Okumura, A.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Ormes, J. F.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa.
[Paneque, D.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Razzano, M.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Razzaque, S.] NYCB Real Time Comp Inc, New York, NY 11560 USA.
[Roth, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Schaal, M.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Siskind, E. J.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain.
[Strong, A. W.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain.
[Takeuchi, Y.] Univ Roma Tor Vergata, Dipartmento Fis, I-00133 Rome, Italy.
RP Ackermann, M (reprint author), DESY, D-15738 Zeuthen, Germany.
EM funk@slac.stanford.edu; warit.mit@mahidol.ac.th; imos@stanford.edu
RI Di Venere, Leonardo/C-7619-2017; Reimer, Olaf/A-3117-2013; Morselli,
Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015;
giglietto, nicola/I-8951-2012; Gomez-Vargas, German/C-7138-2015;
Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Torres,
Diego/O-9422-2016; Johannesson, Gudlaugur/O-8741-2015; Loparco,
Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano,
Fabio/O-8934-2015; Orlando, E/R-5594-2016
OI Di Venere, Leonardo/0000-0003-0703-824X; Reimer,
Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk,
Stefan/0000-0002-2012-0080; giglietto, nicola/0000-0002-9021-2888;
Moskalenko, Igor/0000-0001-6141-458X; Torres, Diego/0000-0002-1522-9065;
Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco,
Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672;
Gargano, Fabio/0000-0002-5055-6395;
FU NASA [NNX11AQ06 G, NNX13AC47 G]; K.A. Wallenberg Foundation; Italian
Ministry of Education, University and Research (MIUR)
[FIRB-2012-RBFR12PM1 F]
FX The Fermi LAT Collaboration acknowledges support from a number of
agencies and institutes for both the 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 gratefully acknowledged.
I. V. M. acknowledges support from NASA Grants No. NNX11AQ06 G and No.
NNX13AC47 G. Royal Swedish Academy of Sciences Research Fellow J.
Conrad, funded by a grant from the K.A. Wallenberg Foundation, NASA
Postdoctoral Program Fellow S. Guiriec, USA. M. Razzano Funded by
Contract No. FIRB-2012-RBFR12PM1 F from the Italian Ministry of
Education, University and Research (MIUR).
NR 33
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PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 17
PY 2014
VL 112
IS 15
AR 151103
DI 10.1103/PhysRevLett.112.151103
PG 7
WC Physics, Multidisciplinary
SC Physics
GA AF3FQ
UT WOS:000334597300003
PM 24785023
ER
PT J
AU Li, Y
Thompson, DWJ
Stephens, GL
Bony, S
AF Li, Ying
Thompson, David W. J.
Stephens, Graeme L.
Bony, Sandrine
TI A global survey of the instantaneous linkages between cloud vertical
structure and large-scale climate
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; GENERAL-CIRCULATION MODEL; TROPICAL DEEP
CONVECTION; EQUATORIAL PLANETARY-WAVES; BREWER-DOBSON CIRCULATION; 1998
EL-NINO; BOUNDARY-LAYER; ANNUAL CYCLE; A-TRAIN; MARINE STRATOCUMULUS
C1 [Li, Ying; Thompson, David W. J.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bony, Sandrine] Univ Paris 06, CNRS, Meteorol Dynam Lab, IPSL, Paris, France.
RP Li, Y (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
EM yingli@atmos.colostate.edu
RI Thompson, David/F-9627-2012;
OI Bony, Sandrine/0000-0002-4791-4438
FU CloudSAT via NASA JPL; NSF Climate Dynamics program
FX We are indebted to Bjorn Stevens, Mark Zelinka, and Robert Wood for
providing comments and suggestions. We would also like to thank Hui Su
and two anonymous referees for their thorough reviews and insightful
comments, which have led to considerable improvement in this work. Y.L.
is funded by CloudSAT via NASA JPL and the NSF Climate Dynamics program.
DWJT is funded by the NSF Climate Dynamics program.
NR 142
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U1 2
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2014
VL 119
IS 7
BP 3770
EP 3792
DI 10.1002/2013JD020669
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF7PZ
UT WOS:000334908300009
ER
PT J
AU Li, JLF
Lee, WL
Waliser, DE
Neelin, JD
Stachnik, JP
Lee, T
AF Li, J. -L. F.
Lee, W. -L.
Waliser, D. E.
Neelin, J. David
Stachnik, Justin P.
Lee, Tong
TI Cloud-precipitation-radiation-dynamics interaction in global climate
models: A snow and radiation interaction sensitivity experiment
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID COMMUNITY ATMOSPHERE MODEL; IN-SITU; ECMWF; CIRCULATIONS; FEEDBACKS;
SATELLITE; PACIFIC; SYSTEM; RADAR; OCEAN
C1 [Li, J. -L. F.; Waliser, D. E.; Stachnik, Justin P.; Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Lee, W. -L.] Acad Sinica, RCEC, Taipei, Taiwan.
[Neelin, J. David] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
RP Li, JLF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Juilin.F.Li@jpl.nasa.gov
RI Stachnik, Justin/A-5609-2015
FU NASA Making Earth System Data Records for Use in Research Environments
(MEaSUREs); Earth Science Data Records Uncertainty (ESDR-ERR); NOAA
[NA11OAR4310099]; National Aeronautics and Space Administration
FX We thank Akio Arakawa at UCLA, Sun Won, Qing Yue, Seungwon Lee, Eric
Fetzer, and Bin Guan at JPL as well as H.-H. Hsu at Academia Sinica,
Taiwan, for useful comments. This work has been supported in part by the
NASA Making Earth System Data Records for Use in Research Environments
(MEaSUREs) and Earth Science Data Records Uncertainty (ESDR-ERR)
programs and in part by the NOAA NA11OAR4310099 (J.D.N.). The
contributions by D.E.W. and J.L.L. 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.
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2014
VL 119
IS 7
BP 3809
EP 3824
DI 10.1002/2013JD021038
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF7PZ
UT WOS:000334908300011
ER
PT J
AU Shindell, D
Racherla, P
Milly, G
AF Shindell, Drew
Racherla, Pavan
Milly, George
TI Reply to comment by Laprise on "The added value to global model
projections of climate change by dynamical downscaling: A case study
over the continental U. S. using the GISS-ModelE2 and WRF models"
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
C1 [Shindell, Drew; Racherla, Pavan; Milly, George] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Shindell, D (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM drew.t.shindell@nasa.gov
RI Shindell, Drew/D-4636-2012
NR 6
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2014
VL 119
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BP 3882
EP 3885
DI 10.1002/2013JD020732
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF7PZ
UT WOS:000334908300015
ER
PT J
AU Muhlbauer, A
Ackerman, TP
Comstock, JM
Diskin, GS
Evans, SM
Lawson, RP
Marchand, RT
AF Muhlbauer, Andreas
Ackerman, Thomas P.
Comstock, Jennifer M.
Diskin, Glenn S.
Evans, Stuart M.
Lawson, R. Paul
Marchand, Roger T.
TI Impact of large-scale dynamics on the microphysical properties of
midlatitude cirrus
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CLOUD PARTICLE ENSEMBLES; RADAR OBSERVATIONS; ICE SUPERSATURATION;
SPARTICUS CAMPAIGN; SIZE SPECTRA; A-TRAIN; AIRCRAFT; PARAMETERIZATIONS;
CLIMATOLOGY; TEMPERATURE
C1 [Muhlbauer, Andreas; Ackerman, Thomas P.] Univ Washington, Joint Inst Study Atmosphere & Oceans, Seattle, WA 98195 USA.
[Ackerman, Thomas P.; Evans, Stuart M.; Marchand, Roger T.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Comstock, Jennifer M.] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Diskin, Glenn S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Lawson, R. Paul] Spec Inc, Boulder, CO USA.
RP Muhlbauer, A (reprint author), Univ Washington, Joint Inst Study Atmosphere & Oceans, Seattle, WA 98195 USA.
EM andreasm@atmos.washington.edu
RI Muhlbauer, Andreas/A-4493-2015;
OI Evans, Stuart/0000-0002-1873-0752
FU National Science Foundation (NSF) [1144017]; Joint Institute for the
Study of the Atmosphere and Ocean (JISAO) under NOAA [NA10OAR4320148,
2138]; Department of Energy (DOE) Atmospheric Measurement Program
FX Andreas Muhlbauer and Thomas P. Ackerman acknowledge funding received by
the National Science Foundation (NSF) under grant 1144017. This
publication is partially funded by the Joint Institute for the Study of
the Atmosphere and Ocean (JISAO) under NOAA Cooperative Agreement
NA10OAR4320148, Contribution 2138. Jennifer Comstock was supported by
the Department of Energy (DOE) Atmospheric Measurement Program. We thank
Ann M. Fridlind (NASA-GISS) for stimulating discussions on an earlier
version of the manuscript and highly appreciate comments and suggestions
from three anonymous reviewers that helped to improve the clarity and
presentation of the manuscript.
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SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2014
VL 119
IS 7
BP 3976
EP 3996
DI 10.1002/2013JD020035
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF7PZ
UT WOS:000334908300021
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: Part III. Using combined PCA to compare spatiotemporal
variability of MODIS, MISR, and OMI aerosol optical depth
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; RUSSIAN WILDFIRES; EASTERN FINLAND; AERONET;
INSTRUMENT; PRODUCTS; TRENDS; INDIA; LAND; ENSO
C1 [Li, Jing; Carlson, Barbara E.; Lacis, Andrew A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Li, Jing] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
RP Li, J (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM jl2862@columbia.edu
FU NASA [509496.02.08.04.24]
FX The authors would like to thank the MODIS, MISR, and OMI team for
providing the AOD data used in this study. We thank the AERONET for
providing the reference data. Thanks are also given to the anonymous
reviewers for providing helpful comments and suggestions. The study is
funded by NASA grant 509496.02.08.04.24. Jing Li is funded by the NASA
Postdoctoral Program (NPP).
NR 53
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PI WASHINGTON
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SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2014
VL 119
IS 7
BP 4017
EP 4042
DI 10.1002/2013JD020538
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF7PZ
UT WOS:000334908300023
ER
PT J
AU Kiemle, C
Kawa, SR
Quatrevalet, M
Browell, EV
AF Kiemle, C.
Kawa, S. R.
Quatrevalet, M.
Browell, E. V.
TI Performance simulations for a spaceborne methane lidar mission
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ATMOSPHERIC CO2; MU-M; REFLECTANCE; SURFACE; COLUMN; SENSITIVITY;
RETRIEVALS; VALIDATION; CH4
C1 [Kiemle, C.; Quatrevalet, M.] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Phys Atmosphare, Oberpfaffenhofen, Germany.
[Kawa, S. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Browell, E. V.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Kiemle, C (reprint author), Deutsch Zentrum Luft & Raumfahrt DLR, Inst Phys Atmosphare, Oberpfaffenhofen, Germany.
EM Christoph.Kiemle@dlr.de
FU MERLIN scientific advisory group
FX Valuable contributions to this work came from Sebastian Bretl (DLR) and
from Jim Abshire and Clark Weaver (both NASA). We acknowledge the
support of the MERLIN scientific advisory group headed by the principal
investigators Gerhard Ehret (DLR) and Pierre Flamant (LMD).
NR 28
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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 APR 16
PY 2014
VL 119
IS 7
BP 4365
EP 4379
DI 10.1002/2013JD021253
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF7PZ
UT WOS:000334908300041
ER
PT J
AU Jaross, G
Bhartia, PK
Chen, G
Kowitt, M
Haken, M
Chen, Z
Xu, P
Warner, J
Kelly, T
AF Jaross, Glen
Bhartia, Pawan K.
Chen, Grace
Kowitt, Mark
Haken, Michael
Chen, Zhong
Xu, Philippe
Warner, Jeremy
Kelly, Thomas
TI OMPS Limb Profiler instrument performance assessment
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SCATTER MEASUREMENTS; OSIRIS INSTRUMENT; ODIN SATELLITE; O-3 PROFILES;
SUITE OMPS; SCIAMACHY; RETRIEVAL; ALGORITHM; MISSION; SENSOR
C1 [Jaross, Glen; Bhartia, Pawan K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Chen, Grace; Kowitt, Mark; Haken, Michael; Chen, Zhong; Warner, Jeremy; Kelly, Thomas] Sci Syst & Applicat Inc, Lanham, MD USA.
[Xu, Philippe] Sci Applicat Int Corp, Beltsville, MD USA.
RP Jaross, G (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM glen.jaross@nasa.gov
RI Bhartia, Pawan/A-4209-2016
OI Bhartia, Pawan/0000-0001-8307-9137
NR 26
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U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2014
VL 119
IS 7
BP 4399
EP 4412
DI 10.1002/2013JD020482
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF7PZ
UT WOS:000334908300043
ER
PT J
AU Seftor, CJ
Jaross, G
Kowitt, M
Haken, M
Li, J
Flynn, LE
AF Seftor, C. J.
Jaross, G.
Kowitt, M.
Haken, M.
Li, J.
Flynn, L. E.
TI Postlaunch performance of the Suomi National Polar-orbiting Partnership
Ozone Mapping and Profiler Suite (OMPS) nadir sensors
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID INSTRUMENT
C1 [Seftor, C. J.; Kowitt, M.; Haken, M.; Li, J.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Jaross, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Flynn, L. E.] NOAA, College Pk, MD USA.
RP Seftor, CJ (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM colin.seftor@ssaihq.com
RI Flynn, Lawrence/B-6321-2009
OI Flynn, Lawrence/0000-0001-6856-2614
NR 19
TC 15
Z9 15
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 APR 16
PY 2014
VL 119
IS 7
BP 4413
EP 4428
DI 10.1002/2013JD020472
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF7PZ
UT WOS:000334908300044
ER
PT J
AU Zhao, H
Li, X
Blake, JB
Fennell, JF
Claudepierre, SG
Baker, DN
Jaynes, AN
Malaspina, DM
Kanekal, SG
AF Zhao, H.
Li, X.
Blake, J. B.
Fennell, J. F.
Claudepierre, S. G.
Baker, D. N.
Jaynes, A. N.
Malaspina, D. M.
Kanekal, S. G.
TI Peculiar pitch angle distribution of relativistic electrons in the inner
radiation belt and slot region
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE pitch angle distribution; radiation belt electrons; inner radiation
belt; slot region; plasmasphere; wave-particle interaction
ID VAN-ALLEN BELT; SOLAR-WIND; MAGNETOSONIC WAVES; DIFFUSION; STORM; DST;
MAGNETOSPHERE; PREDICTION; INDEXES; MODEL
AB The relativistic electrons in the inner radiation belt have received little attention in the past due to sparse measurements and unforgiving contamination from the inner belt protons. The high-quality measurements of the Magnetic Electron Ion Spectrometer instrument onboard Van Allen Probes provide a great opportunity to investigate the dynamics of relativistic electrons in the low L region. In this letter, we report the newly unveiled pitch angle distribution (PAD) of the energetic electrons with minima at 90 degrees near the magnetic equator in the inner belt and slot region. Such a PAD is persistently present throughout the inner belt and appears in the slot region during storms. One hypothesis for 90 degrees minimum PADs is that off 90 degrees electrons are preferentially heated by chorus waves just outside the plasmapause (which can be at very low L during storms) and/or fast magnetosonic waves which exist both inside and outside the plasmasphere.
Key Points
Peculiar pitch angle distribution in the inner belt and slot region is reported Pitch angle distribution with minimum at 90 degrees persists in inner belt Chorus/fast magnetosonic wave heating is suggested as a possible mechanism
C1 [Zhao, H.; Li, X.; Baker, D. N.; Jaynes, A. N.; Malaspina, D. M.] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Zhao, H.; Li, X.] Univ Colorado Boulder, Dept Aerosp Engn Sci, Boulder, CO USA.
[Blake, J. B.; Fennell, J. F.; Claudepierre, S. G.] Aerosp Corp, Los Angeles, CA 90009 USA.
[Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zhao, H (reprint author), Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
EM hong.zhao@colorado.edu
FU NSF (CubeSat program) [AGSW 0940277]; NASA [NNX10AQ48G, NAS5-01072]
FX We would like to thank Richard Selesnick and Mike Temerin, Lauren Blum,
Quintin Schiller, and Sam Califf for helpful discussions. This work is
mainly supported by NSF (CubeSat program) grant AGSW 0940277, NASA grant
NNX10AQ48G, and NASA contract NAS5-01072 (Van Allen Probes mission). We
thank the World Data Center for Geomagnetism, Kyoto, for providing Dst
and AE indices. The predicted Dst and AE indices are available at
http://lasp.colorado.edu/space_weather/dsttemerin/dsttemerin.html.
NR 35
TC 17
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U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2014
VL 41
IS 7
BP 2250
EP 2257
DI 10.1002/2014GL059725
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AF8RJ
UT WOS:000334983000003
ER
PT J
AU Mazarico, E
Barker, MK
Neumann, GA
Zuber, MT
Smith, DE
AF Mazarico, Erwan
Barker, Michael K.
Neumann, Gregory A.
Zuber, Maria T.
Smith, David E.
TI Detection of the lunar body tide by the Lunar Orbiter Laser Altimeter
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Moon; tide; LOLA; crossover
ID RECONNAISSANCE ORBITER; MISSION; GRAIL; MOON
AB The Lunar Orbiter Laser Altimeter instrument onboard the Lunar Reconnaissance Orbiter spacecraft collected more than 5 billion measurements in the nominal 50km orbit over similar to 10,000 orbits. The data precision, geodetic accuracy, and spatial distribution enable two-dimensional crossovers to be used to infer relative radial position corrections between tracks to better than similar to 1m. We use nearly 500,000 altimetric crossovers to separate remaining high-frequency spacecraft trajectory errors from the periodic radial surface tidal deformation. The unusual sampling of the lunar body tide from polar lunar orbit limits the size of the typical differential signal expected at ground track intersections to similar to 10cm. Nevertheless, we reliably detect the topographic tidal signal and estimate the associated Love number h(2) to be 0.03710.0033, which is consistent with but lower than recent results from lunar laser ranging.
C1 [Mazarico, Erwan; Zuber, Maria T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Mazarico, Erwan; Barker, Michael K.; Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Barker, Michael K.] Sigma Space, Lanham, MD USA.
RP Mazarico, E (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
EM mazarico@mit.edu
RI Mazarico, Erwan/N-6034-2014; Neumann, Gregory/I-5591-2013
OI Mazarico, Erwan/0000-0003-3456-427X; Neumann,
Gregory/0000-0003-0644-9944
FU NASA [NNX09AM53G, NNG09HP18C]
FX This work was supported by NASA grants NNX09AM53G and NNG09HP18C. We
thank the LRO project and the LOLA Engineering and Science teams. We
also thank T. Sabaka for his advice and assistance with the least
squares inversion. The authors thank C.K. Shum and J.G. Williams for
their constructive comments.
NR 23
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U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2014
VL 41
IS 7
BP 2282
EP 2288
DI 10.1002/2013GL059085
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA AF8RJ
UT WOS:000334983000007
ER
PT J
AU Desai, SD
Ray, RD
AF Desai, Shailen D.
Ray, Richard D.
TI Consideration of tidal variations in the geocenter on satellite
altimeter observations of ocean tides
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ocean tides; geocenter; altimetry
ID MISSION; EARTH; DEFORMATION; JASON-1
AB Tidal geocenter motion has been previously ignored when developing ocean tide models from satellite altimetry. Accounting for tidal geocenter motion is necessary because the best orbit determinations for altimetric satellites position sea-surface heights relative to the center of mass of the total Earth system, including the ocean tides. But the ocean tides are presumed relative to the Earth's crust and thus are effectively relative to the center of figure. By accounting for this effect, we find improved agreement between an altimeter-based ocean tide model and bottom pressure recorder observations. The variance of differences between these two observations is reduced by 31% and 43% for the two tidal constituents with the largest contributions to geocenter variations, O-1 and K-1, respectively. With this accommodation the predicted contribution from altimeter-based ocean tide models to geocenter variations is amplified by 15-22%, providing improved agreement with observations, especially for the K-1 component.
Key Points
Tidal geocenter motion impacts ocean tide observations from satellite altimetry Geocenter motion has been previously ignored in altimetric ocean tide solutions Consistency between models and observations markedly improved for K1 and O1
C1 [Desai, Shailen D.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Ray, Richard D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Desai, SD (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM shailen.desai@jpl.nasa.gov
RI Ray, Richard/D-1034-2012
FU National Aeronautics and Space Administration; National Aeronautics and
Space Administration's Ocean Surface Topography project
FX The bottom-pressure-record data used in this study are available as
supporting information to Ray [2013] at
http://onlinelibrary.wiley.com/doi/10.1002/jgrc.20336/suppinfo. SDD
performed the work described in this paper at the Jet Propulsion
Laboratory, California Institute of Technology under contract with the
National Aeronautics and Space Administration. RDR was supported by the
National Aeronautics and Space Administration's Ocean Surface Topography
project.
NR 19
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U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2014
VL 41
IS 7
BP 2454
EP 2459
DI 10.1002/2014GL059614
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA AF8RJ
UT WOS:000334983000029
ER
PT J
AU Mlynczak, MG
Hunt, LA
Mertens, CJ
Marshall, BT
Russell, JM
Woods, T
Thompson, RE
Gordley, LL
AF Mlynczak, Martin G.
Hunt, Linda A.
Mertens, Christopher J.
Marshall, B. Thomas
Russell, James M., III
Woods, Thomas
Thompson, R. Earl
Gordley, Larry L.
TI Influence of solar variability on the infrared radiative cooling of the
thermosphere from 2002 to 2014
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE thermosphere; radiative cooling; solar cycle; carbon dioxide; nitric
oxide
ID NITRIC-OXIDE; SABER EXPERIMENT; STORMS; MESOSPHERE; EMISSION
AB Infrared radiative cooling of the thermosphere by carbon dioxide (CO2, 15 mu m) and by nitric oxide (NO, 5.3 mu m) has been observed for 12years by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument on the Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics satellite. For the first time we present a record of the two most important thermospheric infrared cooling agents over a complete solar cycle. SABER has documented dramatic variability in the radiative cooling on time scales ranging from days to the 11 year solar cycle. Deep minima in global mean vertical profiles of radiative cooling are observed in 2008-2009. Current solar maximum conditions, evidenced in the rates of radiative cooling, are substantially weaker than prior maximum conditions in 2002-2003. The observed changes in thermospheric cooling correlate well with changes in solar ultraviolet irradiance and geomagnetic activity during the prior maximum conditions. NO and CO2 combine to emit 7x10(18) more Joules annually at solar maximum than at solar minimum.
Key Points
First record of thermospheric IR cooling rates over a complete solar cycle IR cooling in current solar maximum conditions much weaker than prior maximum Variability in thermospheric IR cooling observed on scale of days to 11 years
C1 [Mlynczak, Martin G.; Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Hunt, Linda A.] SSAI, Hampton, VA USA.
[Marshall, B. Thomas; Thompson, R. Earl; Gordley, Larry L.] G&A Tech Software, Newport News, VA USA.
[Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Woods, Thomas] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM m.g.mlynczak@nasa.gov
FU NASATIMED project; NASA Living with a Star program
FX The authors would like to thank the NASATIMED project and the NASA
Living with a Star program for support. The data reported in this letter
may be obtained directly by sending an email request to
m.g.mlynczak@nasa.gov.
NR 21
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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 APR 16
PY 2014
VL 41
IS 7
BP 2508
EP 2513
DI 10.1002/2014GL059556
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA AF8RJ
UT WOS:000334983000037
ER
PT J
AU Durand, M
Neal, J
Rodriguez, E
Andreadis, KM
Smith, LC
Yoon, Y
AF Durand, Michael
Neal, Jeffrey
Rodriguez, Ernesto
Andreadis, Konstantinos M.
Smith, Laurence C.
Yoon, Yeosang
TI Estimating reach-averaged discharge for the River Severn from
measurements of river water surface elevation and slope
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE River discharge; Remote sensing; Inverse methods; Open channels;
Bayesian analysis
ID DATA ASSIMILATION; INVERSE PROBLEM; FLOOD WAVE; PARAMETER; UNCERTAINTY;
ROUGHNESS; AMAZON; STATE; OPTIMIZATION; INFORMATION
AB An algorithm is presented that calculates a best estimate of river bathymetry, roughness coefficient, and discharge based on input measurements of river water surface elevation (h) and slope (S) using the Metropolis algorithm in a Bayesian Markov Chain Monte Carlo scheme, providing an inverse solution to the diffusive approximation to the shallow water equations. This algorithm has potential application to river Is and S measurements from the forthcoming Surface Water and Ocean Topography (SWOT) satellite mission. The algorithm was tested using in situ data as a proxy for satellite measurements along a 22.4 km reach of the River Severn, UK. First, the algorithm was run with gage measurements of h and S during a small, in-bank event in June 2007. Second, the algorithm was run with measurements of Is and S estimated from four remote sensing images during a major out-of-bank flood event in July 2007. River width was assumed to be known for both events. Algorithm-derived estimates of river bathymetry were validated using in situ measurements, and estimates of roughness coefficient were compared to those used in an operational hydraulic model. Algorithm-derived estimates of river discharge were evaluated using gaged discharge. For the in-bank event, when lateral inflows from smaller tributaries were assumed to be known, the method provided an accurate discharge estimate (10% RMSE). When lateral inflows were assumed unknown, discharge RMSE increased to 36%. Finally, if just one of the three river reaches was assumed to be have known bathymetry, solutions for bathymetry, roughness and discharge for all three reaches were accurately retrieved, with a corresponding discharge RMSE of 15.6%. For the out-of-bank flood event, the lateral inflows were unknown, and the final discharge RMSE was 19%. These results suggest that it should be possible to estimate river discharge via SWOT observations of river water surface elevation, slope and width. (c) 2014 Elsevier B.V. All rights reserved.
C1 [Durand, Michael] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
[Durand, Michael] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
[Neal, Jeffrey] Univ Bristol, Sch Geog Sci, Bristol, Avon, England.
[Rodriguez, Ernesto; Andreadis, Konstantinos M.] CALTECH, Pasadena, CA 91011 USA.
[Rodriguez, Ernesto; Andreadis, Konstantinos M.] NASA, Jet Prop Lab, Pasadena, CA 91011 USA.
[Smith, Laurence C.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA.
[Durand, Michael; Yoon, Yeosang] Ohio State Univ, Columbus, OH 43210 USA.
RP Durand, M (reprint author), Ohio State Univ, 275 Mendenhall Lab,125 South Oval Mall, Columbus, OH 43210 USA.
EM durand.8@osu.edu
RI Neal, Jeffrey/C-8723-2009; Durand, Michael/D-2885-2013; Smith,
Laurence/E-7785-2012
OI Neal, Jeffrey/0000-0001-5793-9594; Smith, Laurence/0000-0001-6866-5904
FU NASA Physical Oceanography Grant [NNX10AE96G]
FX We thank the Environment Agency of England and Wales for providing river
cross-section and gauging stations data. This work was supported by NASA
Physical Oceanography Grant NNX10AE96G. Three anonymous reviewers helped
improve the quality of the manuscript.
NR 46
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U1 0
U2 22
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-1694
EI 1879-2707
J9 J HYDROL
JI J. Hydrol.
PD APR 16
PY 2014
VL 511
BP 92
EP 104
DI 10.1016/j.jhydrol.2013.12.050
PG 13
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA AG2VJ
UT WOS:000335274900010
ER
PT J
AU Wang, K
Day, JMD
Korotev, RL
Zeigler, RA
Moynier, F
AF Wang, Kun
Day, James M. D.
Korotev, Randy L.
Zeigler, Ryan A.
Moynier, Frederic
TI Iron isotope fractionation during sulfide-rich felsic partial melting in
early planetesimals
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE iron isotopes; GRA 06128/9; brachinites; brachinite-like achondrites;
partial melting; sulfide melts
ID EARLY SOLAR-SYSTEM; UNEQUILIBRATED ORDINARY CHONDRITES; PARENT-BODY;
MAGMATIC DIFFERENTIATION; CONTINENTAL-CRUST; OSMIUM ISOTOPE; FE
ISOTOPES; METEORITES; ORIGIN; ACCRETION
AB New Fe isotope data of feldspar-rich meteorites Graves Nunataks 06128 and 06129 (GRA 06128/9) reveal that they are the only known examples of crustal materials with isotopically light Fe isotope compositions (delta Fe-66 = -0.08 +/- 0.06 parts per thousand; delta Fe-66 is defined as the per mule deviation of a sample's Fe-56/Fe-54 ratio from the IRMM-014 standard) in the Solar System. In contrast, associated brachinites, as well as brachinite-like achondrites, have Fe isotope compositions (delta Fe-56 = +0.01 +/- 0.02 parts per thousand) that are isotopically similar to carbonaceous chondrites and the bulk terrestrial mantle. In order to understand the cause of Fe isotope variations in the GRA 06128/9 and brachinite parent body, we also report the Fe isotope compositions of metal, silicate and sulfide fractions from three ordinary chondrites (Semarkona, Kernouve, Saint-Severin). Metals from ordinary chondrites are enriched in the heavier isotopes of Fe (average delta Fe-56 = 0.15 parts per thousand), sulfide fractions are enriched in the lighter isotopes of Fe (average delta Fe-56 = -0.14 parts per thousand), and the delta Fe-56 values of the silicates are coincident with that of the bulk rock (average delta Fe-56 = 0.03 parts per thousand).
The enrichment of light isotopes of Fe isotopes in GRA 06128/9 is consistent with preferential melting of sulfides in precursor chondritic source materials leading to the formation of Fe-S-rich felsic melts. Conceptual models show that melt generation to form a GRA 06128/9 parental melt occurred prior to the onset of higher-temperature basaltic melting (<1200 degrees C) in a volatile-rich precursor and led to the generation of buoyant felsic melt with a strong Fe-S signature. These models not only reveal the origin of enrichment in light isotopes of Fe for GRA 06128/9, but are also consistent with petrological and geochemical observations, experimental studies for the origin of Fe-S-rich felsic melts, and for the cessation of early melting on some asteroidal parent bodies because of the effective removal of the major radioactive heat-source, Al-26. The mode of origin for GRA 06128/9 contrasts strongly with crust formation on Earth, the Moon. Mars and other asteroids, where mantle differentiation and/or oxygen activity are the major controls on crustal Fe isotope compositions. (C)2014 Elsevier B.V. All rights reserved.
C1 [Wang, Kun; Korotev, Randy L.; Moynier, Frederic] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
[Wang, Kun; Korotev, Randy L.; Moynier, Frederic] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Day, James M. D.] Univ Calif San Diego, Scripps Inst Oceanog, Geosci Res Div, La Jolla, CA 92093 USA.
[Zeigler, Ryan A.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate Acquisit, Houston, TX 77058 USA.
[Moynier, Frederic] Univ Paris Diderot, Inst Phys Globe Paris, F-75238 Paris 05, France.
RP Wang, K (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA.
EM kunwang@fas.harvard.edu
FU NASA Earth and Space Science Fellowship [NNX12AL84H]; NASA
Cosmochemistry program [NNX12AH70G, NNX12AH75G]
FX Nicolas Dauphas is thanked for generously providing access to the
MC-ICP-MS facility at the University of Chicago and Corliss K. Sio is
thanked for assistance with analyses at the facility. This work was
supported by the NASA Earth and Space Science Fellowship (NNX12AL84H to
K.W.) and by funding from the NASA Cosmochemistry program (NNX12AH70G to
F.M. and NNX12AH75G to J.M.D.D.). F.M. thanks a Chaire d'Excellence
Sorbonne Paris Cite #IDEX13C445. Helen Williams and Paolo Sossi are
thanked for their careful and constructive reviews and Tim Elliott is
thanked for his thoughtful editorial handling.
NR 65
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U1 3
U2 11
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 APR 15
PY 2014
VL 392
BP 124
EP 132
DI 10.1016/j.epsl.2014.02.022
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CA8BI
UT WOS:000349141100014
ER
PT J
AU Woodworth, AA
Neudeck, PG
Sayir, A
Sola, F
Dudley, M
Raghothamachar, B
AF Woodworth, A. A.
Neudeck, P. G.
Sayir, A.
Sola, F.
Dudley, M.
Raghothamachar, B.
TI Investigation of single crystal 4H-SiC growth by the Solvent-Laser
Heated Floating Zone technique
SO JOURNAL OF CRYSTAL GROWTH
LA English
DT Article
DE X-ray diffraction; X-ray topography; Floating zone technique; Traveling
solvent zone growth; Silicon carbide; Wide band gap semiconductor
ID SILICON-CARBIDE; DEVICES; SI; TEMPERATURE; MECHANISM; LAYERS
AB The Solvent-Laser Heated Floating Zone (solvent-LHFZ) growth technique has been implemented to grow long single crystal silicon carbide (SiC) fibers. This technique combines the long fiber growth ability of laser heated floating zone with crystal growth by traveling solvent method's ability to grow single crystal SiC. This paper presents a complete look at the initial SiC growth study by solvent-LtFZ. This study shows that solvent-LHFZ readily grows single crystal SiC, growth rates are a function of both growth temperature and carbon concentration in the crystal growth source material, solvent incorporation is a function of carbon concentration in the crystal growth source material, and that an ordered growth front must be achieved in order to grow a long single crystal SiC fiber. (C) 2014 Elsevier B.V. All rights reserved
C1 [Woodworth, A. A.; Neudeck, P. G.; Sayir, A.; Sola, F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Dudley, M.; Raghothamachar, B.] SUNY Stony Brook, Dept Mat Sci & Engn, Stony Brook, NY 11794 USA.
RP Woodworth, AA (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM andrew.a.woodworth@nasa.gov
FU NASA Vehicle Systems Safety Technologies Project in the Aviation Safety
Program; US Department of Energy Vehicle Technology Program via Space
Act Agreement [SAA3-1048, DE-EE0001093/ 001]; Susan Rogers (DOE); U.S.
Department of Energy, Office of Science, Office of Basic Energy Sciences
[DE-ACO298CH10886]
FX NASA Postdoctoral Program Fellowship supported by NASA Vehicle Systems
Safety Technologies Project in the Aviation Safety Program, US
Department of Energy Vehicle Technology Program via Space Act Agreement
(SAA3-1048) (DOE IA # DE-EE0001093/ 001) monitored by Susan Rogers
(DOE). Use of the National Synchrotron Light Source, Brookhaven National
Laboratoiy, was supported by the U.S. Department of Energy, Office of
Science, Office of Basic Energy Sciences, under Contract no.
DE-ACO298CH10886. Technical help from Fredric Dynys, David Spry and
Andrew Trunek (NASA), J. Anthony Powell (Sest Inc.), Thomas Sabo
(0AI/Case Western Reserve University), Michelle Mrdenovich-Hill and Beth
Osborn (Sierra Lobo) and Charles Blaha (Jacobs Technologies) is
gratefully acknowledged.
NR 37
TC 2
Z9 2
U1 4
U2 21
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0248
EI 1873-5002
J9 J CRYST GROWTH
JI J. Cryst. Growth
PD APR 15
PY 2014
VL 392
BP 34
EP 40
DI 10.1016/j.jcrysgro.2013.12.050
PG 7
WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied
SC Crystallography; Materials Science; Physics
GA AG9WS
UT WOS:000335771300006
ER
PT J
AU Peng, ZX
Mahoney, JJ
Vanderkluysen, L
Hooper, PR
AF Peng, Zhan X.
Mahoney, John J.
Vanderkluysen, Loyc
Hooper, Peter R.
TI Sr, Nd and Pb isotopic and chemical compositions of central Deccan Traps
lavas and relation to southwestern Deccan stratigraphy
SO JOURNAL OF ASIAN EARTH SCIENCES
LA English
DT Article
DE Deccan Traps; Geochemistry; Large igneous provinces; Chemical
stratigraphy
ID FLOOD-BASALT PROVINCE; GEOCHEMICAL STRATIGRAPHY; INDIA; MAHABALESHWAR;
FLOWS; ELEMENT; SECTION; GEOLOGY; ORIGIN; SYSTEM
AB Sr, Nd and Pb isotopic compositions, and major and trace element abundances of lavas in five central Deccan Traps sections are generally very similar to those of lavas in the southwestern Deccan (Western Ghats escarpment). The combination of strong isotopic and chemical similarities between lavas of the two regions indicates that they shared a closely similar petrogenesis. Our results indicate that, unlike many lavas in the northeastern Deccan, most of the lavas studied in the central Deccan sections can be grouped into different stratigraphic members and chemical types (CTs) belonging to four formations (Thakurvadi, Bhimashankar, Khandala, and Poladpur) present in the type sections of the Western Ghats. Bhimashankar- and Thakurvadi-type lavas are found in a section near Outram, whereas only Khandala-type lavas make up the Mhaishmal, Ellora and Ajanta sections to the east, and only Poladpur-type lavas are present in the easternmost section at Lonar. This west-east sequence is the same as that seen going upward in the Western Ghats stratigraphy, except that Bushe-type lavas, which are located stratigraphically between the Khandala and Poladpur formations in the Western Ghats, have not been found in this study. Overall, our results indicate that the Khandala and Poladpur formations extend over west-east distances of more than 300 km, and some individual members (e.g., the Dhak Dongar) may extend over as much as 500 km. The regional dip from Igatpuri in the southwest to Lonar in the east-central Deccan is less than 0.5 degrees to the east, which is similar to the southward regional dip in the southwestern Deccan. Near-horizontal flows in the central and southwestern Deccan areas suggest that post-Deccan tectonic activity has had limited effects on the studied area. Large volumes of basaltic lavas derived from eruptive centers in the western Deccan may have covered both the central and southwestern Deccan areas. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Peng, Zhan X.] NASA, Lyndon B Johnson Space Ctr, Engn & Sci Contract Grp, Houston, TX 77058 USA.
[Mahoney, John J.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA.
[Vanderkluysen, Loyc] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Hooper, Peter R.] Washington State Univ, Dept Geol, Pullman, WA 99162 USA.
RP Peng, ZX (reprint author), NASA, Lyndon B Johnson Space Ctr, Engn & Sci Contract Grp, Houston, TX 77058 USA.
EM zxpeng37@gmail.com; loyc@asu.edu
OI Vanderkluysen, Loyc/0000-0001-8263-1604
FU U.S. National Science Foundation [EAR-8816192, EAR-9104897, EAR-9418168]
FX We thank N. Chatterjee and M. Bodas for their careful reviews of the
manuscript, and handling editor H. Sheth for his many helpful comments.
We are grateful to K. Spencer for his help with laboratory work. ZXP and
LV are forever grateful to co-authors J. Mahoney and P. Hooper, who were
admirable teachers and mentors; we regret that they could not see this
work to its completion and hope to honor their memory with the
publication of this work. This study was funded by U.S. National Science
Foundation grants EAR-8816192, EAR-9104897 and EAR-9418168.
NR 47
TC 7
Z9 7
U1 2
U2 10
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1367-9120
EI 1878-5786
J9 J ASIAN EARTH SCI
JI J. Asian Earth Sci.
PD APR 15
PY 2014
VL 84
SI SI
BP 83
EP 94
DI 10.1016/j.jseaes.2013.10.025
PG 12
WC Geosciences, Multidisciplinary
SC Geology
GA AF1NW
UT WOS:000334481600008
ER
PT J
AU Aponte, JC
Tarozo, R
Alexandre, MR
Alexander, CMO
Charnley, SB
Hallmann, C
Summons, RE
Huang, YS
AF Aponte, Jose C.
Tarozo, Rafael
Alexandre, Marcelo R.
Alexander, Conel M. O'D.
Charnley, Steven B.
Hallmann, Christian
Summons, Roger E.
Huang, Yongsong
TI Chirality of meteoritic free and IOM-derived monocarboxylic acids and
implications for prebiotic organic synthesis
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID CIRCULARLY-POLARIZED-LIGHT; STAR-FORMATION REGIONS; AMINO-ACIDS;
MURCHISON METEORITE; ASYMMETRIC AUTOCATALYSIS; CARBONACEOUS METEORITES;
ENANTIOMERIC EXCESSES; MOLECULAR-WEIGHT; DENSE CLOUDS; HOMOCHIRALITY
AB The origin of homochirality and its role in the development of life on Earth are among the most intriguing questions in science. It has been suggested that carbonaceous chondrites seeded primitive Earth with the initial organic compounds necessary for the origin of life. One of the strongest pieces of evidence supporting this theory is that certain amino acids in carbonaceous chondrites display a significant L-enantiomeric excess (ee), similar to those use by terrestrial life. Analyses of ee in meteoritic molecules other than amino acids would shed more light on the origins of homochirality. In this study we investigated the stereochemistry of two groups of compounds: (1) free monocarboxylic acids (MCAs) from CM2 meteorites LON 94101 and Murchison; and (2) the aliphatic side chains present in the insoluble organic matter (IOM) and extracted in the form of monocarboxylic acids (MCAs) from EET 87770 (CR2) and Orgueil (CI1). Contrary to the well-known ee observed for amino acids in meteorites, we found that meteoritic branched free and IOM-derived MCAs with 5-8 carbon atoms are essentially racemic. The racemic nature of these compounds is used to discuss the possible influence of ultraviolet circularly polarized light (UVCPL) and aqueous alterations on the parent body on chirality observed in in carbonaceous chondrites. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Aponte, Jose C.; Tarozo, Rafael; Huang, Yongsong] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Alexandre, Marcelo R.] Univ Fed Sergipe, Dept Quim, BR-49100000 Sao Cristovao, SE, Brazil.
[Alexander, Conel M. O'D.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Charnley, Steven B.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Hallmann, Christian; Summons, Roger E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Hallmann, Christian] Max Planck Inst Biogeochem, D-28359 Bremen, Germany.
[Hallmann, Christian] Univ Bremen, MARUM, D-28359 Bremen, Germany.
RP Aponte, JC (reprint author), NASA, Goddard Space Flight Ctr, NASA Postdoctoral Program, Greenbelt, MD 20771 USA.
EM jose.c.aponte@nasa.gov; yongsong_huang@brown.edu
RI Alexander, Conel/N-7533-2013
OI Alexander, Conel/0000-0002-8558-1427
FU NSF; NASA; NASA Astrobiology and Exobiology Grant [NNX09AM82G]; Agouron
Institute; NASA Astrobiology Institute [NNA08CN84A]
FX US Antarctic meteorite samples are recovered by the Antarctic Search for
Meteorites (ANSMET) program which has been funded by NSF and NASA, and
characterized and curated by the Department of Mineral Sciences of the
Smithsonian Institution and Astromaterials Curation Office at NASA
Johnson Space Center. This research was entirely supported by NASA
Astrobiology and Exobiology Grant NNX09AM82G to YH. JCA is grateful to
the NASA Postdoctoral Program Administered by Oak Ridge Associated
Universities. RES and CH were supported by the Agouron Institute and the
NASA Astrobiology Institute (NNA08CN84A). JCA and YH acknowledge Michel
Nuevo for helpful discussions during preparation of the manuscript, and
associate editor George Cooper and three anonymous reviewers for their
valuable criticisms during the review process.
NR 65
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Z9 11
U1 2
U2 33
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD APR 15
PY 2014
VL 131
BP 1
EP 12
DI 10.1016/j.gca.2014.01.035
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AD5YS
UT WOS:000333330100001
ER
PT J
AU Danielski, C
Deroo, P
Waldmann, IP
Hollis, MDJ
Tinetti, G
Swain, MR
AF Danielski, C.
Deroo, P.
Waldmann, I. P.
Hollis, M. D. J.
Tinetti, G.
Swain, M. R.
TI 0.94-2.42 mu m GROUND-BASED TRANSMISSION SPECTRA OF THE HOT JUPITER
HD-189733b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; planets and satellites: atmospheres; planets and
satellites: individual (HD-189733b); techniques: spectroscopic
ID EXOPLANET HD 189733B; HUBBLE-SPACE-TELESCOPE;
INFRARED-EMISSION-SPECTRUM; EXTRASOLAR PLANET; SPITZER OBSERVATIONS;
WATER-ABSORPTION; ATMOSPHERIC HAZE; CARBON-MONOXIDE; ORBITAL MOTION;
LINE LISTS
AB We present here new transmission spectra of the hot Jupiter HD-189733b using the SpeX instrument on the NASA Infrared Telescope Facility. We obtained two nights of observations where we recorded the primary transit of the planet in the J, H, and K bands simultaneously, covering a spectral range from 0.94 to 2.42 mu m. We used Fourier analysis and other detrending techniques validated previously on other data sets to clean the data. We tested the statistical significance of our results by calculating the autocorrelation function, and we found that, after the detrending, autocorrelative noise is diminished at most frequencies. Additionally, we repeated our analysis on the out-of-transit data only, showing that the residual telluric contamination is well within the error bars. While these techniques are very efficient when multiple nights of observations are combined together, our results prove that even one good night of observations is enough to provide statistically meaningful data. Our observed spectra are consistent with space-based data recorded in the same wavelength interval by multiple instruments, indicating that ground-based facilities are becoming a viable and complementary option to spaceborne observatories. The best fit to the features in our data was obtained with water vapor. Our error bars are not small enough to address the presence of additional molecules; however, by combining the information contained in other data sets with our results, it is possible to explain all the available observations with a modeled atmospheric spectrum containing water vapor, methane, carbon monoxide, and hazes/clouds.
C1 [Danielski, C.; Waldmann, I. P.; Hollis, M. D. J.; Tinetti, G.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Deroo, P.; Swain, M. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Danielski, C (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
EM camilla@star.ucl.ac.uk
OI Hollis, Morgan/0000-0002-8058-9075
NR 59
TC 12
Z9 12
U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2014
VL 785
IS 1
AR 35
DI 10.1088/0004-637X/785/1/35
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300035
ER
PT J
AU Helgason, K
Cappelluti, N
Hasinger, G
Kashlinsky, A
Ricotti, M
AF Helgason, K.
Cappelluti, N.
Hasinger, G.
Kashlinsky, A.
Ricotti, M.
TI THE CONTRIBUTION OF z less than or similar to 6 SOURCES TO THE SPATIAL
COHERENCE IN THE UNRESOLVED COSMIC NEAR-INFRARED AND X-RAY BACKGROUNDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; dark ages; reionization; first stars;
diffuse radiation; large-scale structure of universe
ID ACTIVE GALACTIC NUCLEI; HALO OCCUPATION DISTRIBUTION; QUASAR LUMINOSITY
FUNCTION; STAR-FORMATION HISTORY; LARGE-SCALE STRUCTURE; POINT-SOURCE
CATALOG; INTERGALACTIC MEDIUM; REDSHIFT SURVEY; THEORETICAL-MODELS;
GALAXY POPULATION
AB A spatial clustering signal has been established in Spitzer/IRAC measurements of the unresolved cosmic near-infrared background (CIB) out to large angular scales, similar to 1 degrees. This CIB signal, while significantly exceeding the contribution from the remaining known galaxies, was further found to be coherent at a highly statistically significant level with the unresolved soft cosmic X-ray background (CXB). This measurement probes the unresolved CXB to very faint source levels using deep near-IR source subtraction. We study contributions from extragalactic populations at low to intermediate redshifts to the measured positive cross-power signal of the CIB fluctuations with the CXB. We model the X-ray emission from active galactic nuclei (AGNs), normal galaxies, and hot gas residing in virialized structures, calculating their CXB contribution including their spatial coherence with all infrared emitting counterparts. We use a halo model framework to calculate the auto and cross-power spectra of the unresolved fluctuations based on the latest constraints of the halo occupation distribution and the biasing of AGNs, galaxies, and diffuse emission. At small angular scales (less than or similar to 1'), the 4.5 mu m versus 0.5-2 keV coherence can be explained by shot noise from galaxies and AGNs. However, at large angular scales (similar to 10'), we find that the net contribution from the modeled populations is only able to account for similar to 3% of the measured CIBxCXB cross-power. The discrepancy suggests that the CIBxCXB signal originates from the same unknown source population producing the CIB clustering signal out to similar to 1 degrees.
C1 [Helgason, K.; Ricotti, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Helgason, K.; Kashlinsky, A.] NASA Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Cappelluti, N.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Cappelluti, N.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Hasinger, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Kashlinsky, A.] SSAI, Lanham, MD 20706 USA.
RP Helgason, K (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM kari@astro.umd.edu
OI Cappelluti, Nico/0000-0002-1697-186X
FU NASA Headquarters under the NASA Earth and Space Sciences Fellowship
Program [NNX11AO05H]
FX K.H.acknowledges useful discussions with R.Arendt, A.Ferrara, B.Lehmer,
and R.Mushotzky.This work was supported by NASA Headquarters under the
NASA Earth and Space Sciences Fellowship Program Grant-NNX11AO05H.
NR 79
TC 5
Z9 5
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2014
VL 785
IS 1
AR 38
DI 10.1088/0004-637X/785/1/38
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300038
ER
PT J
AU Jontof-Hutter, D
Lissauer, JJ
Rowe, JF
Fabrycky, DC
AF Jontof-Hutter, Daniel
Lissauer, Jack J.
Rowe, Jason F.
Fabrycky, Daniel C.
TI KEPLER-79'S LOW DENSITY PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (KOI-152, Kepler-79); techniques:
photometric
ID TRANSIT TIMING OBSERVATIONS; SUB-NEPTUNE EXOPLANETS; SUPER-EARTH;
LIGHT-CURVE; ASTROPHYSICAL PARAMETERS; EXTRASOLAR PLANETS; HOT NEPTUNE;
LOW-MASS; M DWARF; K STAR
AB Kepler-79 (KOI-152) has four planetary candidates ranging in size from 3.5 to 7 times the size of the Earth, in a compact configuration with orbital periods near a 1: 2: 4: 6 chain of commensurability, from 13.5 to 81.1 days. All four planets exhibit transit timing variations with periods that are consistent with the distance of each planet to resonance with its neighbors. We perform a dynamical analysis of the system based on transit timing measurements over 1282 days of Kepler photometry. Stellar parameters are obtained using a combination of spectral classification and the stellar density constraints provided by light curve analysis and orbital eccentricity solutions from our dynamical study. Our models provide tight bounds on the masses of all four transiting bodies, demonstrating that they are planets and that they orbit the same star. All four of Kepler-79's transiting planets have low densities given their sizes, which is consistent with other studies of compact multiplanet transiting systems. The largest of the four, Kepler-79 d (KOI-152.01), has the lowest bulk density yet determined among sub-Saturn mass planets.
C1 [Jontof-Hutter, Daniel; Lissauer, Jack J.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rowe, Jason F.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
RP Jontof-Hutter, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Daniel.S.Jontof-Hutter@nasa.gov
OI Fabrycky, Daniel/0000-0003-3750-0183
FU NASA Postdoctoral Program
FX D.J. gratefully acknowledges the support of the NASA Postdoctoral
Program and thanks Yanqin Wu for a helpful review. We also thank Billy
Quarles and Bill Borucki for helpful discussions of this paper.
NR 50
TC 35
Z9 35
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2014
VL 785
IS 1
AR 15
DI 10.1088/0004-637X/785/1/15
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300015
ER
PT J
AU Lansbury, GB
Alexander, DM
Del Moro, A
Gandhi, P
Assef, RJ
Stern, D
Aird, J
Ballantyne, DR
Balokovic, M
Bauer, FE
Boggs, SE
Brandt, WN
Christensen, FE
Craig, WW
Elvis, M
Grefenstette, BW
Hailey, CJ
Harrison, FA
Hickox, RC
Koss, M
LaMassa, SM
Luo, B
Mullaney, JR
Teng, SH
Urry, CM
Zhang, WW
AF Lansbury, G. B.
Alexander, D. M.
Del Moro, A.
Gandhi, P.
Assef, R. J.
Stern, D.
Aird, J.
Ballantyne, D. R.
Balokovic, M.
Bauer, F. E.
Boggs, S. E.
Brandt, W. N.
Christensen, F. E.
Craig, W. W.
Elvis, M.
Grefenstette, B. W.
Hailey, C. J.
Harrison, F. A.
Hickox, R. C.
Koss, M.
LaMassa, S. M.
Luo, B.
Mullaney, J. R.
Teng, S. H.
Urry, C. M.
Zhang, W. W.
TI NuSTAR OBSERVATIONS OF HEAVILY OBSCURED QUASARS AT z similar to 0.5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; HARD X-RAY; SEYFERT 2
GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; RESOLUTION SPECTRAL
TEMPLATES; XMM-NEWTON OBSERVATIONS; COMPTON-THICK QUASARS; MU-M; TYPE-2
QUASARS
AB We present NuSTAR hard X-ray observations of three Type 2 quasars at z approximate to 0.4-0.5, optically selected from the Sloan Digital Sky Survey. Although the quasars show evidence for being heavily obscured, Compton-thick systems on the basis of the 2-10 keV to [O III] luminosity ratio and multiwavelength diagnostics, their X-ray absorbing column densities (N-H) are poorly known. In this analysis, (1) we study X-ray emission at > 10 keV, where X-rays from the central black hole are relatively unabsorbed, in order to better constrain N-H. (2) We further characterize the physical properties of the sources through broad-band near-UV to mid-IR spectral energy distribution analyses. One of the quasars is detected with NuSTAR at > 8 keV with a no-source probability of < 0.1%, and its X-ray band ratio suggests near Compton-thick absorption with N-H greater than or similar to 5 Chi 10(23) cm(-2). The other two quasars are undetected, and have low X-ray to mid-IR luminosity ratios in both the low-energy (2-10 keV) and high-energy (10-40 keV) X-ray regimes that are consistent with extreme, Compton-thick absorption (N-H greater than or similar to 10(24) cm(-2)). We find that for quasars at z similar to 0.5, NuSTAR provides a significant improvement compared to lower energy (< 10 keV) Chandra and XMM-Newton observations alone, as higher column densities can now be directly constrained.
C1 [Lansbury, G. B.; Alexander, D. M.; Del Moro, A.; Gandhi, P.; Aird, J.; Mullaney, J. R.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Assef, R. J.] Univ Diego Port, Nucl Astron Fac Ingn, Santiago, Chile.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ballantyne, D. R.] Georgia Inst Technol, Ctr Relativist Astrophys, Sch Phys, Atlanta, GA 30332 USA.
[Balokovic, M.; Grefenstette, B. W.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 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.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Koss, M.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland.
[LaMassa, S. M.; Urry, C. M.] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA.
[Teng, S. H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lansbury, GB (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England.
EM g.b.lansbury@durham.ac.uk
RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt,
William/N-2844-2015;
OI Urry, Meg/0000-0002-0745-9792; Boggs, Steven/0000-0001-9567-4224; Koss,
Michael/0000-0002-7998-9581; Brandt, William/0000-0002-0167-2453;
Alexander, David/0000-0002-5896-6313
FU Science and Technology Facilities Council (STFC) [ST/K501979/1,
ST/I001573/1, ST/J003697/1]; Leverhulme Trust; Gemini-CONICYT
[32120009]; NSF AST [1008067]; International Fulbright Science and
Technology Award; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT
1101024, Anillo ACT1101]; Caltech NuSTAR [44A-1092750]; NASA ADP
[NNX10AC99G]; NASA ADAP [NNX12AE38G]; National Science Foundation
[1211096]; Swiss National Science Foundation [PP00P2_ 138979/1]; NASA
[NNG08FD60C]; National Aeronautics and Space Administration; ASI Science
Data Center (ASDC, Italy); California Institute of Technology (USA)
FX We acknowledge financial support from the Science and Technology
Facilities Council (STFC) grants ST/K501979/1 (G.B.L.), ST/I001573/1
(D.M.A. and A.D.M.) and ST/J003697/1 (P.G.), the Leverhulme Trust
(D.M.A. and J.R.M.), Gemini-CONICYT grant 32120009 (R.J.A.), NSF AST
award 1008067 (D.R.B.), the International Fulbright Science and
Technology Award (M.B.), Basal-CATA PFB-06/2007 (F.E.B.), CONICYT-Chile
grant FONDECYT 1101024 (F.E.B.), CONICYT-Chile grant Anillo ACT1101
(F.E.B.), Caltech NuSTAR subcontract 44A-1092750 (W.N.B. and B.L.), NASA
ADP grant NNX10AC99G (W.N.B.and B.L.), NASA ADAP award NNX12AE38G
(R.C.H.), National Science Foundation grant 1211096 (R.C.H.), and Swiss
National Science Foundation grant PP00P2_ 138979/1 (M.K.). We thank the
referee for the constructive comments, which helped improve our study.
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).
NR 88
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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 APR 10
PY 2014
VL 785
IS 1
AR 17
DI 10.1088/0004-637X/785/1/17
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300017
ER
PT J
AU Liu, Y
Hoeksema, JT
Bobra, M
Hayashi, K
Schuck, PW
Sun, X
AF Liu, Y.
Hoeksema, J. T.
Bobra, M.
Hayashi, K.
Schuck, P. W.
Sun, X.
TI MAGNETIC HELICITY IN EMERGING SOLAR ACTIVE REGIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: interior; Sun: magnetic fields; Sun: photosphere; sunspots
ID ELECTRIC-CURRENT HELICITY; FORCE-FREE FIELDS; VECTOR MAGNETOGRAMS; FLUX
TUBES; ENERGY; TWIST; SUN; INJECTION; CORONA; EVOLUTION
AB Using vector magnetic field data from the Helioseismic and Magnetic Imager instrument aboard the Solar Dynamics Observatory, we study magnetic helicity injection into the corona in emerging active regions (ARs) and examine the hemispheric helicity rule. In every region studied, photospheric shearing motion contributes most of the helicity accumulated in the corona. In a sample of 28 emerging ARs, 17 follow the hemisphere rule (61% +/- 18% at a 95% confidence interval). Magnetic helicity and twist in 25 ARs (89% +/- 11%) have the same sign. The maximum magnetic twist, which depends on the size of an AR, is inferred in a sample of 23 emerging ARs with a bipolar magnetic field configuration.
C1 [Liu, Y.; Hoeksema, J. T.; Bobra, M.; Hayashi, K.; Sun, X.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Schuck, P. W.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Liu, Y (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
RI Sun, Xudong/M-3245-2013
OI Sun, Xudong/0000-0003-4043-616X
FU NASA to Stanford University [NAS5-02139]; Heliophysics Guest
Investigators grant
FX The authors thank the team members who have made great contributions to
the Solar Dynamics Observatory mission and for their hard work. The
authors thank the anonymous referee for comments and suggestions that
improved this paper. This investigation was supported by NASA Contract
NAS5-02139 (HMI) to Stanford University. This study was also supported
by NASA's Living with a Star program grant and Heliophysics Guest
Investigators grant.
NR 51
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U2 2
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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 APR 10
PY 2014
VL 785
IS 1
AR 13
DI 10.1088/0004-637X/785/1/13
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300013
ER
PT J
AU Luna, M
Knizhnik, K
Muglach, K
Karpen, J
Gilbert, H
Kucera, TA
Uritsky, V
AF Luna, M.
Knizhnik, K.
Muglach, K.
Karpen, J.
Gilbert, H.
Kucera, T. A.
Uritsky, V.
TI OBSERVATIONS AND IMPLICATIONS OF LARGE-AMPLITUDE LONGITUDINAL
OSCILLATIONS IN A SOLAR FILAMENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun : corona; Sun : filaments, prominences; Sun : flares; Sun :
oscillations
ID MAGNETIC-STRUCTURE; PERIODIC MOTION; ACTIVE-REGION; POLAR CROWN;
PROMINENCES; SDO/AIA; EVOLUTION; DYNAMICS; THREADS; CHANNEL
AB On 2010 August 20, an energetic disturbance triggered large-amplitude longitudinal oscillations in a nearby filament. The triggering mechanism appears to be episodic jets connecting the energetic event with the filament threads. In the present work, we analyze this periodic motion in a large fraction of the filament to characterize the underlying physics of the oscillation as well as the filament properties. The results support our previous theoretical conclusions that the restoring force of large-amplitude longitudinal oscillations is solar gravity, and the damping mechanism is the ongoing accumulation of mass onto the oscillating threads. Based on our previous work, we used the fitted parameters to determine the magnitude and radius of curvature of the dipped magnetic field along the filament, as well as the mass accretion rate onto the filament threads. These derived properties are nearly uniform along the filament, indicating a remarkable degree of cohesiveness throughout the filament channel. Moreover, the estimated mass accretion rate implies that the footpoint heating responsible for the thread formation, according to the thermal nonequilibrium model, agrees with previous coronal heating estimates. We estimate the magnitude of the energy released in the nearby event by studying the dynamic response of the filament threads, and discuss the implications of our study for filament structure and heating.
C1 [Luna, M.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Luna, M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Knizhnik, K.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Knizhnik, K.; Muglach, K.; Karpen, J.; Gilbert, H.; Kucera, T. A.; Uritsky, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Muglach, K.] ARTEP Inc, Ellicott City, MD 21042 USA.
[Uritsky, V.] Catholic Univ Amer, NASA GSFC, Greenbelt, MD 20771 USA.
RP Luna, M (reprint author), Inst Astrofis Canarias, E-38200 Tenerife, Spain.
OI Kucera, Therese/0000-0001-9632-447X
FU Spanish Ministry of Economy [AYA2011-24808, CSD2007-00050]; NASA's
Heliophysics LWS and SR programs; National Science Foundation [0962619];
LWS TRT Program; European Research Council [277829]; Catholic University
of America
FX M.L. gratefully acknowledges partial financial support by the Spanish
Ministry of Economy through projects AYA2011-24808 and CSD2007-00050.
This work contributes to the deliverables identified in FP7 European
Research Council grant agreement 277829, "Magnetic Connectivity through
the Solar Partially Ionized Atmosphere" (PI: E. Khomenko). K.K.
acknowledges support for this work by a coop agreement between the
Catholic University of America and NASA Goddard Space Flight Center,
sponsored by NASA's Heliophysics LWS and SR programs. K.M. gratefully
acknowledges funding from the National Science Foundation via grant #
0962619. SDO is a mission for NASA's Living With a Star program. H.G.,
J.K., and T.K. also thank the LWS TR&T Program for support. We also
thank S. Antiochos, I. Arregui, A. Asensio-Ramos, J. L. Ballester, C. R.
DeVore, A. D iaz, A. Lopez-Ariste, F. Moreno-Insertis, R. Oliver, D.
Orozco-Suarez, and J. Terradas for helpful discussions and suggestions.
NR 42
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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 APR 10
PY 2014
VL 785
IS 1
AR 79
DI 10.1088/0004-637X/785/1/79
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300079
ER
PT J
AU Nelson, T
Chomiuk, L
Roy, N
Sokoloski, JL
Mukai, K
Krauss, MI
Mioduszewski, AJ
Rupen, MP
Weston, J
AF Nelson, Thomas
Chomiuk, Laura
Roy, Nirupam
Sokoloski, J. L.
Mukai, Koji
Krauss, Miriam I.
Mioduszewski, Amy J.
Rupen, Michael P.
Weston, Jennifer
TI THE 2011 OUTBURST OF RECURRENT NOVA T PYX: RADIO OBSERVATIONS REVEAL THE
EJECTA MASS AND HINT AT COMPLEX MASS LOSS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE novae, cataclysmic variables; radio continuum : stars; stars :
individual (T Pyxidis); white dwarfs
ID CLASSICAL NOVAE; SPECTROSCOPIC EVOLUTION; CATACLYSMIC VARIABLES; MERLIN
OBSERVATIONS; ORBITAL PERIOD; RS-OPHIUCHI; PYXIDIS; EMISSION; PHASE;
SHELL
AB Despite being the prototype of its class, T Pyx is arguably the most unusual and poorly understood recurrent nova. Here, we use radio observations from the Karl G. Jansky Very Large Array to trace the evolution of the ejecta over the course of the 2011 outburst of T Pyx. The radio emission is broadly consistent with thermal emission from the nova ejecta. However, the radio flux began rising surprisingly late in the outburst, indicating that the bulk of the radio- emitting material was either very cold, or expanding very slowly, for the first similar to 50 days of the outburst. Considering a plausible range of volume filling factors and geometries for the ejecta, we find that the high peak flux densities of the radio emission require a massive ejection of (1-30) Chi 10(-5) M-circle dot. This ejecta mass is much higher than the values normally associated with recurrent novae, and is more consistent with a nova on a white dwarf well below the Chandrasekhar limit.
C1 [Nelson, Thomas] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Chomiuk, Laura] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Chomiuk, Laura; Roy, Nirupam; Krauss, Miriam I.; Mioduszewski, Amy J.; Rupen, Michael P.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Sokoloski, J. L.; Weston, Jennifer] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Mukai, Koji] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Mukai, Koji] CRESST, Greenbelt, MD 20771 USA.
[Mukai, Koji] NASA GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
RP Nelson, T (reprint author), Univ Minnesota, Sch Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA.
EM tnelson@physics.umn.edu
FU National Science Foundation [AST-1217778]
FX We are grateful to H. Uthas, R. Williams, M. Shara, J. Patterson, S.
Starrfield, M. Kato and D. Prialnik for illuminating discussions, and to
the anonymous referee for their feedback on this work. We thank NRAO for
the generous allocation of director's discretionary time that made this
work possible. We are also grateful to the VLA commissioning team,
including J. McMullin, J. Wrobel, E. Momjian, L. Sjouwerman, and G. van
Moorsel, for their assistance in the acquisition of this data set. The
National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. This work was carried out while L. Chomiuk and N. Roy
were Jansky Fellows of the National Radio Astronomy Observatory. J.L.S.
and J.W. acknowledge support from the National Science Foundation
through award AST-1217778. Finally, we acknowledge with thanks the
variable star observations from the AAVSO International Database
contributed by observers worldwide and used in this research.
NR 64
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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 APR 10
PY 2014
VL 785
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AR 78
DI 10.1088/0004-637X/785/1/78
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300078
ER
PT J
AU Obenberger, KS
Hartman, JM
Taylor, GB
Craig, J
Dowell, J
Helmboldt, JF
Henning, PA
Schinzel, FK
Wilson, TL
AF Obenberger, K. S.
Hartman, J. M.
Taylor, G. B.
Craig, J.
Dowell, J.
Helmboldt, J. F.
Henning, P. A.
Schinzel, F. K.
Wilson, T. L.
TI LIMITS ON GAMMA-RAY BURST PROMPT RADIO EMISSION USING THE LWA1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst COLFAML; general
ID BLACK-HOLE; SEARCH; PULSES; SKY; AFTERGLOWS; TELESCOPE; SPECTRUM;
DENSITY; MISSION; SCALE
AB As a backend to the first station of the Long Wavelength Array (LWA1), the Prototype All Sky Imager has been imaging the sky >-26 degrees declination during 34 gamma-ray bursts (GRBs) between 2012 January and 2013 May. Using this data, we were able to put the most stringent limits to date on prompt low-frequency emission from GRBs. While our limits depend on the zenith angle of the observed GRB, we estimate a 1 sigma rms sensitivity of 68, 65, and 70 Jy for 5 s integrations at 37.9, 52.0, and 74.0 MHz at zenith. These limits are relevant for pulses >= 5 s and are limited by dispersion smearing. For 5 s pulses, we are limited to dispersion measures (DMs) <= 220, 570, and 1600 pc cm(-3) for the frequencies above. For pulses lasting longer than 5 s, the DM limits increase linearly with the duration of the pulse. We also report two interesting transients, which are, as of yet, of unknown origin and are not coincident with any known GRBs. For general transients, we give rate density limits of <= 7.5 Chi 10(-3), 2.9 Chi 10(-2), and 1.4 Chi 10(-2) yr(-1) deg(-2) with pulse energy densities > 1.3 Chi 10(-22), 1.1 Chi 10(-22), and 1.4 Chi 10(-22) J m(-2) Hz(-1) and pulse widths of 5 s at the frequencies given above.
C1 [Obenberger, K. S.; Taylor, G. B.; Craig, J.; Dowell, J.; Henning, P. A.; Schinzel, F. K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
[Hartman, J. M.] NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Helmboldt, J. F.; Wilson, T. L.] US Naval Res Lab, Washington, DC 20375 USA.
RP Obenberger, KS (reprint author), Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
RI Helmboldt, Joseph/C-8105-2012
FU Office of Naval Research [N00014-07-C-0147]; National Science Foundation
[AST-1139963, AST-1139974]
FX Construction of the LWA1 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 grants AST-1139963 and AST-1139974 of the University
Radio Observatory program.
NR 38
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U2 0
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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 APR 10
PY 2014
VL 785
IS 1
AR 27
DI 10.1088/0004-637X/785/1/27
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300027
ER
PT J
AU Parchevsky, KV
Zhao, J
Hartlep, T
Kosovichev, AG
AF Parchevsky, K. V.
Zhao, J.
Hartlep, T.
Kosovichev, A. G.
TI VERIFICATION OF THE HELIOSEISMOLOGY TRAVEL-TIME MEASUREMENT TECHNIQUE
AND THE INVERSION PROCEDURE FOR SOUND SPEED USING ARTIFICIAL DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun COLFAML; helioseismology; Sun COLFAML; oscillations; sunspots; waves
ID ACOUSTIC-WAVE-FIELD; DISTANCE HELIOSEISMOLOGY; NUMERICAL SIMULATIONS;
3-DIMENSIONAL INVERSION; HOLOGRAPHY; SUNSPOTS; SUN; PERTURBATIONS;
SENSITIVITY; FLOWS
AB We performed three-dimensional numerical simulations of the solar surface acoustic wave field for the quiet Sun and for three models with different localized sound-speed perturbations in the interior with deep, shallow, and two-layer structures. We used the simulated data generated by two solar acoustics codes that employ the same standard solar model as a background model, but utilize different integration techniques and different models of stochastic wave excitation. Acoustic travel times were measured using a time-distance helioseismology technique, and compared with predictions from ray theory frequently used for helioseismic travel-time inversions. It is found that the measured travel-time shifts agree well with the helioseismic theory for sound-speed perturbations, and for the measurement procedure with and without phase-speed filtering of the oscillation signals. This testing verifies the whole measuring-filtering-inversion procedure for static sound-speed anomalies with small amplitude inside the Sun outside regions of strong magnetic field. It is shown that the phase-speed filtering, frequently used to extract specific wave packets and improve the signal-to-noise ratio, does not introduce significant systematic errors. Results of the sound-speed inversion procedure show good agreement with the perturbation models in all cases. Due to its smoothing nature, the inversion procedure may overestimate sound-speed variations in regions with sharp gradients of the sound-speed profile.
C1 [Parchevsky, K. V.; Zhao, J.; Hartlep, T.; Kosovichev, A. G.] Stanford Univ, HEPL, Stanford, CA 94305 USA.
[Hartlep, T.] NASA, Ames Res Ctr, BAER Inst, Mountain View, CA 94043 USA.
[Kosovichev, A. G.] Big Bear Solar Observ, Big Bear City, CA 92314 USA.
[Kosovichev, A. G.] New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA.
[Kosovichev, A. G.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine.
RP Parchevsky, KV (reprint author), Stanford Univ, HEPL, Stanford, CA 94305 USA.
EM akosovichev@solar.stanford.edu
RI Zhao, Junwei/A-1177-2007;
OI Hartlep, Thomas/0000-0002-5062-9507
FU NASA Living With a Star TR T program
FX This work was partially supported by the NASA Living With a Star TR& T
program. The numerical simulations were carried out using the NASA Ames
Research Center and XSEDE computational resources.
NR 32
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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 APR 10
PY 2014
VL 785
IS 1
AR 40
DI 10.1088/0004-637X/785/1/40
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300040
ER
PT J
AU Pesnell, WD
Bryans, P
AF Pesnell, W. D.
Bryans, P.
TI THE TIME-DEPENDENT CHEMISTRY OF COMETARY DEBRIS IN THE SOLAR CORONA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; comets: individual (C/2011 W3); Sun: corona; Sun:
general
ID EXTREME-ULTRAVIOLET EMISSION; SUN-GRAZING COMET; X-RAY; SUNGRAZING
COMETS; ATOMIC DATABASE; MISSION; SOHO; SPECTRA; CHIANTI; LINES
AB Recent improvements in solar observations have greatly progressed the study of sungrazing comets. They can now be imaged along the entirety of their perihelion passage through the solar atmosphere, revealing details of their composition and structure not measurable through previous observations in the less volatile region of the orbit further from the solar surface. Such comets are also unique probes of the solar atmosphere. The debris deposited by sungrazers is rapidly ionized and subsequently influenced by the ambient magnetic field. Measuring the spectral signature of the deposited material highlights the topology of the magnetic field and can reveal plasma parameters such as the electron temperature and density. Recovering these variables from the observable data requires a model of the interaction of the cometary species with the atmosphere through which they pass. The present paper offers such a model by considering the time-dependent chemistry of sublimated cometary species as they interact with the solar radiation field and coronal plasma. We expand on a previous simplified model by considering the fully time-dependent solutions of the emitting species' densities. To compare with observations, we consider a spherically symmetric expansion of the sublimated material into the corona and convert the time-dependent ion densities to radial profiles. Using emissivities from the CHIANTI database and plasma parameters derived from a magnetohydrodynamic simulation leads to a spatially dependent emission spectrum that can be directly compared with observations. We find our simulated spectra to be consistent with observation.
C1 [Pesnell, W. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bryans, P.] NASA, ADNET Syst Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Pesnell, WD (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
RI Pesnell, William/D-1062-2012
OI Pesnell, William/0000-0002-8306-2500
NR 32
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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 APR 10
PY 2014
VL 785
IS 1
AR 50
DI 10.1088/0004-637X/785/1/50
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300050
ER
PT J
AU Revalski, M
Nowak, D
Wiita, PJ
Wehrle, AE
Unwin, SC
AF Revalski, Mitchell
Nowak, Dawid
Wiita, Paul J.
Wehrle, Ann E.
Unwin, Stephen C.
TI INVESTIGATING THE VARIABILITY OF ACTIVE GALACTIC NUCLEI USING COMBINED
MULTI-QUARTER KEPLER DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; galaxies: active; galaxies: jets; galaxies:
photometry; galaxies: Seyfert; quasars: general
ID RAPID OPTICAL VARIABILITY; DAMPED RANDOM-WALK; MODELS; QUASARS
AB We used photometry from the Kepler satellite to characterize the variability of four radio-loud active galactic nuclei (AGNs) on timescales from years to minutes. The Kepler satellite produced nearly continuous high precision data sets which provided better temporal coverage than possible with ground based observations. We have now accumulated 11 quarters of data, eight of which were reported in our previous paper. In addition to constructing power spectral densities (PSDs) and characterizing the variability of the last three quarters, we have linked together the individual quarters using a multiplicative scaling process, providing data sets spanning similar to 2.8 yr with >98% coverage at a 30 minute sampling rate. We compute PSDs on these connected data sets that yield power law slopes at low frequencies in the approximate range of -1.5 to -2.0, with white noise seen at higher frequencies. These PSDs are similar to those of both the individual quarters and to those of ground-based optical observations of other AGNs. We also have explored a PSD binning method intended to reduce a bias toward shallow slope fits by evenly distributing the points within the PSDs. This tends to steepen the computed PSD slopes, especially when the low frequencies are relatively poorly fit. We detected flares lasting several days in which the brightness increased by similar to 15%-20% in one object, as well a smaller flare in another. Two AGNs showed only small, similar to 1%-2%, fluctuations in brightness.
C1 [Revalski, Mitchell; Nowak, Dawid; Wiita, Paul J.] Coll New Jersey, Dept Phys, Ewing, NJ 08628 USA.
[Wehrle, Ann E.] Space Sci Inst, Boulder, CO 80301 USA.
[Unwin, Stephen C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Revalski, M (reprint author), Coll New Jersey, Dept Phys, POB 7718, Ewing, NJ 08628 USA.
EM revalsm1@tcnj.edu
OI Wiita, Paul/0000-0002-1029-3746
FU NASA Kepler Guest Observer Program [NNX11B90G, NNX12AC83G]; Mentored
Undergraduate Summer Experience (MUSE) Program at TCNJ; National
Aeronautics and Space Administration
FX We thank Victoria Calafut for assistance in developing original PSD
codes and scripts. We are grateful to Paolo Di Lorenzo, Daniel Silano,
and Daniel Sprague for developing codes and techniques used in Paper I
that were also employed here. We thank Brandon Kelly for providing his
DRW code and the anonymous referee for comments which improved the scope
of this manuscript. We acknowledge support from the NASA Kepler Guest
Observer Program through grants NNX11B90G and NNX12AC83G (PI: A.E.W.)
and from the 2013 Mentored Undergraduate Summer Experience (MUSE)
Program at TCNJ (PI: P.J.W.) during which most of this work was carried
out. 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 24
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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 APR 10
PY 2014
VL 785
IS 1
AR 60
DI 10.1088/0004-637X/785/1/60
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300060
ER
PT J
AU Stacy, A
Bromm, V
AF Stacy, Athena
Bromm, Volker
TI THE FIRST STARS: A LOW-MASS FORMATION MODE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: theory; dark ages, reionization, first stars; stars:
formation; stars: Population III
ID POPULATION-III STARS; EXTREMELY METAL-POOR; PRIMORDIAL STELLAR
EVOLUTION; SUPERMASSIVE BLACK-HOLES; ASYMPTOTIC GIANT BRANCH; LAMBDA-CDM
UNIVERSE; DARK-MATTER HALOES; SMALL-SCALE DYNAMO; HIGH-REDSHIFT; GALAXY
FORMATION
AB We perform numerical simulations of the growth of a Population III stellar system under photodissociating feedback. We start from cosmological initial conditions at z = 100, self-consistently following the formation of a minihalo at z = 15 and the subsequent collapse of its central gas to high densities. The simulations resolve scales as small as similar to 1 AU, corresponding to gas densities of 1016 cm(-3). Using sink particles to represent the growing protostars, we evolve the stellar system for the next 5000 yr. We find that this emerging stellar group accretes at an unusually low rate compared with minihalos which form at earlier times (z = 20-30), or with lower baryonic angular momentum. The stars in this unusual system will likely reach masses ranging from <1 M-circle dot to similar to 5 M-circle dot by the end of their main-sequence lifetimes, placing them in the mass range for which stars will undergo an asymptotic giant branch (AGB) phase. Based upon the simulation, we predict the rare existence of Population III stars that have survived to the present day and have been enriched by mass overflow from a previous AGB companion.
C1 [Stacy, Athena] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stacy, Athena] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Bromm, Volker] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Bromm, Volker] Univ Texas Austin, Texas Cosmol Ctr, Austin, TX 78712 USA.
RP Stacy, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM athena.stacy@berkeley.edu
FU JWST Postdoctoral Fellowship through the NASA Postdoctoral Program
(NPP); NASA through Astrophysics Theory and Fundamental Physics Program
[NNX09AJ33G]; NSF [AST-1009928]
FX The authors thank the anonymous referee who helped them improve this
manuscript. A.S. is grateful for support from the JWST Postdoctoral
Fellowship through the NASA Postdoctoral Program (NPP). V.B.
acknowledges support from NASA through Astrophysics Theory and
Fundamental Physics Program grant NNX09AJ33G and from NSF through grant
AST-1009928. 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.
NR 126
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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 APR 10
PY 2014
VL 785
IS 1
AR 73
DI 10.1088/0004-637X/785/1/73
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300073
ER
PT J
AU Teng, SH
Brandt, WN
Harrison, FA
Luo, B
Alexander, DM
Bauer, FE
Boggs, SE
Christensen, FE
Comastri, A
Craig, WW
Fabian, AC
Farrah, D
Fiore, F
Gandhi, P
Grefenstette, BW
Hailey, CJ
Hickox, RC
Madsen, KK
Ptak, AF
Rigby, JR
Risaliti, G
Saez, C
Stern, D
Veilleux, S
Walton, DJ
Wik, DR
Zhang, WW
AF Teng, Stacy H.
Brandt, W. N.
Harrison, F. A.
Luo, B.
Alexander, D. M.
Bauer, F. E.
Boggs, S. E.
Christensen, F. E.
Comastri, A.
Craig, W. W.
Fabian, A. C.
Farrah, D.
Fiore, F.
Gandhi, P.
Grefenstette, B. W.
Hailey, C. J.
Hickox, R. C.
Madsen, K. K.
Ptak, A. F.
Rigby, J. R.
Risaliti, G.
Saez, C.
Stern, D.
Veilleux, S.
Walton, D. J.
Wik, D. R.
Zhang, W. W.
TI NuSTAR REVEALS AN INTRINSICALLY X-RAY WEAK BROAD ABSORPTION LINE QUASAR
IN THE ULTRALUMINOUS INFRARED GALAXY MARKARIAN 231
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; quasars: individual (Mrk 231); X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; ADVECTION-DOMINATED
ACCRETION; DIGITAL SKY SURVEY; XMM-NEWTON; SEYFERT-GALAXIES; CHANDRA
SURVEY; EMISSION-LINE; LOCAL ULIRGS; ENERGY-DISTRIBUTIONS
AB We present high-energy (3-30 keV) NuSTAR observations of the nearest quasar, the ultraluminous infrared galaxy (ULIRG) Markarian 231 (Mrk 231), supplemented with new and simultaneous low-energy (0.5-8 keV) data from Chandra. The source was detected, though at much fainter levels than previously reported, likely due to contamination in the large apertures of previous non-focusing hard X-ray telescopes. The full band (0.5-30 keV) X-ray spectrum suggests the active galactic nucleus (AGN) in Mrk 231 is absorbed by a patchy and Compton-thin (N-H similar to 1.2(-0.3)(+0.3) Chi 10(23) cm(-2)) column. The intrinsic X-ray luminosity (L0.5-30 keV similar to 1.0 Chi 10(43) erg s(-1)) is extremely weak relative to the bolometric luminosity where the 2-10 keV to bolometric luminosity ratio is similar to 0.03% compared to the typical values of 2%-15%. Additionally, Mrk 231 has a low X-ray-to-optical power law slope (alpha(OX) similar to -1.7). It is a local example of a low-ionization broad absorption line quasar that is intrinsically X-ray weak. The weak ionizing continuum may explain the lack of mid-infrared [O Iv], [Ne v], and [Ne vI] fine-structure emission lines which are present in sources with otherwise similar AGN properties. We argue that the intrinsic X-ray weakness may be a result of the super-Eddington accretion occurring in the nucleus of this ULIRG, and may also be naturally related to the powerful wind event seen in Mrk 231, a merger remnant escaping from its dusty cocoon.
C1 [Teng, Stacy H.; Rigby, J. R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Harrison, F. A.; Grefenstette, B. W.; Madsen, K. K.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Alexander, D. M.; Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Comastri, A.] INAF Osserv Astron Bologna, I-40127 Bologna, Italy.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Fabian, A. C.] Inst Astron, Cambridge CB3 0HA, England.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Fiore, F.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Ptak, A. F.; Wik, D. R.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Risaliti, G.] INAF Osserv Astrofis Arcetri, I-50125 Florence, Italy.
[Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Veilleux, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
RP Teng, SH (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
EM stacy.h.teng@nasa.gov
RI Rigby, Jane/D-4588-2012; Boggs, Steven/E-4170-2015; Brandt,
William/N-2844-2015; Comastri, Andrea/O-9543-2015;
OI Rigby, Jane/0000-0002-7627-6551; Boggs, Steven/0000-0001-9567-4224;
Brandt, William/0000-0002-0167-2453; Comastri,
Andrea/0000-0003-3451-9970; Risaliti, Guido/0000-0002-3556-977X;
Alexander, David/0000-0002-5896-6313; Fiore,
Fabrizio/0000-0002-4031-4157
FU NASA [NNG08FD60C]; California Institute of Technology; National
Aeronautics and Space Administration; NuSTAR Data Analysis Software
(NuSTARDAS); ASI Science Data Center (ASDC, Italy); California Institute
of Technology (USA); ESA Member States; USA (NASA); Jet Propulsion
Laboratory, Caltech; Jet Propulsion Laboratory, Caltech, under contract
with NASA; NASA Postdoctoral Program (NPP) Fellowship; California
Institute of Technology (Caltech) NuSTAR [44A-1092750]; NASA ADP
[NNX10AC99G]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024,
Anillo ACT1101]; ASI/INAF [I/037/12/0011/13]; STFC [ST/J003697/1]
FX We are grateful to the anonymous referee for providing useful comments
which improved our manuscript. We thank Wayne Baumgartner, Bret Lehmer,
Richard Mushotzky, Jeremy Schnittman, Tahir Yaqoob, and Andreas Zezas
for useful discussions. We would also like to thank Lee Armus who
provided useful comments in the early planning phase of the NuSTAR ULIRG
program. We also thank Roberto Maiolino, David Rupke, and Eckhard Sturm
who are co-investigators of the Chandra program. 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). The scientific results reported in this article are based in part
on observations made by the Chandra X-Ray Observatory and data obtained
from the Chandra Data Archive published previously in cited articles.
This work, in part, made use of observations obtained with XMM-Newton,
an ESA science mission with instruments and contributions directly
funded by ESA Member States and the USA (NASA). We made use of the
NASA/IPAC Extragalactic Database (NED), which is operated by the Jet
Propulsion Laboratory, Caltech, under contract with NASA. S.H.T. is
supported by a NASA Postdoctoral Program (NPP) Fellowship. W.N.B. and
B.L. acknowledge support by California Institute of Technology (Caltech)
NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. F.E.B.
acknowledges support from Basal-CATA (PFB-06/2007) and CONICYT-Chile
(under grants FONDECYT 1101024 and Anillo ACT1101). A.C. acknowledges
support from ASI/INAF grant I/037/12/0011/13. P.G. acknowledges support
from STFC grant reference ST/J003697/1.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
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DI 10.1088/0004-637X/785/1/19
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300019
ER
PT J
AU Tomsick, JA
Gotthelf, EV
Rahoui, F
Assef, RJ
Bauer, FE
Bodaghee, A
Boggs, SE
Christensen, FE
Craig, WW
Fornasini, FM
Grindlay, J
Hailey, CJ
Harrison, FA
Krivonos, R
Natalucci, L
Stern, D
Zhang, WW
AF Tomsick, John A.
Gotthelf, Eric V.
Rahoui, Farid
Assef, Roberto J.
Bauer, Franz E.
Bodaghee, Arash
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Fornasini, Francesca M.
Grindlay, Jonathan
Hailey, Charles J.
Harrison, Fiona A.
Krivonos, Roman
Natalucci, Lorenzo
Stern, Daniel
Zhang, William W.
TI NuSTAR J163433-4738.7: A FAST X-RAY TRANSIENT IN THE GALACTIC PLANE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: stellar content; stars: variables: general; surveys; X-rays:
individual NuSTAR J1634334738.7); X-rays: stars
ID MILKY-WAY; BINARIES; SUPERFLARE; EVOLUTION; CATALOG; MISSION; GALAXY;
SWIFT; FLARE; WIND
AB During hard X-ray observations of the Norma spiral arm region by the Nuclear Spectroscopic Telescope Array (NuSTAR) in 2013 February, a new transient source, NuSTAR J163433-4738.7, was detected at a significance level of 8s in the 3-10 keV bandpass. The source is consistent with having a constant NuSTAR count rate over a period of 40 ks and is also detected simultaneously by Swift at lower significance. The source is not significantly detected by NuSTAR, Swift, or Chandra in the days before or weeks after the discovery of the transient, indicating that the strong X-ray activity lasted between similar to 0.5 and 1.5 days. Near-infrared imaging observations were carried out before and after the X-ray activity, but we are not able to identify the counterpart. The combined NuSTAR and Swift energy spectrum is consistent with a power law with a photon index of Gamma = 4.1(-1.0)(+1.5) (90% confidence errors), a blackbody with kT = 1.2 +/- 0.3 keV, or a Bremsstrahlung model with kT = 3.0(-1.2)(+2.1) keV. The reduced-chi(2) values for the three models are not significantly different, ranging from 1.23 to 1.44 for 8 degrees of freedom. The spectrum is strongly absorbed with N-Pi = (2.8(-1.4)(+2.3)) x 10(23) cm(-2), (9(-7)(+15)) x 10(22) cm(-2), and (1.7(-0.9)(+1.7)) x 10(23) cm(-2), for the power-law, blackbody, and Bremsstrahlung models, respectively. Although the high column density could be due to material local to the source, it is consistent with absorption from interstellar material along the line of sight at a distance of 11 kpc, which would indicate an X-ray luminosity >10(34) erg s(-1). Although we do not reach a definitive determination of the nature of NuSTAR J163433-4738.7, we suggest that it may be an unusually bright active binary or a magnetar.
C1 [Tomsick, John A.; Bodaghee, Arash; Boggs, Steven E.; Craig, William W.; Fornasini, Francesca M.; Krivonos, Roman] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Gotthelf, Eric V.; Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Rahoui, Farid] European So Observ, D-85748 Garching, Germany.
[Rahoui, Farid] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Assef, Roberto J.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile.
[Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA.
[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.
[Fornasini, Francesca M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Grindlay, Jonathan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Natalucci, Lorenzo] INAF IAPS, Ist Nazl Astrofis, I-00133 Rome, Italy.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Tomsick, JA (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM jtomsick@ssl.berkeley.edu
RI Boggs, Steven/E-4170-2015
OI Boggs, Steven/0000-0001-9567-4224
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
Gemini-CONICYT [32120009]; Basal-CATA [PFB-06/2007]; CONICYT-Chile
through FONDECYT [1101024]; CONICYT-Chile through Gemini-CONICYT
[32120003]; CONICYT-Chile through Anillo [ACT1101]; Italian Space Agency
(ASI) by ASI/INAF grant [I/037/12/0-011/13]
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. The authors
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 (Italy) and the California
Institute of Technology (USA). R.J.A. was supported by Gemini-CONICYT
grant 32120009. F.E.B. was supported by Basal-CATA PFB-06/2007 and
CONICYT-Chile (through FONDECYT 1101024, Gemini-CONICYT 32120003, and
Anillo ACT1101). L.N. wishes to acknowledge the Italian Space Agency
(ASI) for financial support by ASI/INAF grant I/037/12/0-011/13. The
authors thank Harvey Tananbaum for providing Chandra Director's
Discretionary Time for this project. This research has made use of the
SIMBAD database, operated at CDS, Strasbourg, France.
NR 36
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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 APR 10
PY 2014
VL 785
IS 1
AR 4
DI 10.1088/0004-637X/785/1/4
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300004
ER
PT J
AU Younes, G
Kouveliotou, C
van der Horst, AJ
Baring, MG
Granot, J
Watts, AL
Bhat, PN
Collazzi, A
Gehrels, N
Gorgone, N
Gogus, E
Gruber, D
Grunblatt, S
Huppenkothen, D
Kaneko, Y
von Kienlin, A
van der Klis, M
Lin, L
Mcenery, J
van Putten, T
Wijers, RAMJ
AF Younes, G.
Kouveliotou, C.
van der Horst, A. J.
Baring, M. G.
Granot, J.
Watts, A. L.
Bhat, P. N.
Collazzi, A.
Gehrels, N.
Gorgone, N.
Gogus, E.
Gruber, D.
Grunblatt, S.
Huppenkothen, D.
Kaneko, Y.
von Kienlin, A.
van der Klis, M.
Lin, L.
Mcenery, J.
van Putten, T.
Wijers, R. A. M. J.
TI TIME RESOLVED SPECTROSCOPY OF SGR J1550-5418 BURSTS DETECTED WITH
FERMI/GAMMA-RAY BURST MONITOR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars : individual (SGR J1550-5418); stars : magnetars; X-rays : bursts
ID SOFT GAMMA-REPEATERS; MAGNETIZED NEUTRON-STARS; PULSAR 1E 1547.0-5408;
X-RAY; STATISTICAL PROPERTIES; 2009 OUTBURST; GIANT FLARES; SGR-1900+14;
MAGNETARS; EMISSION
AB We report on a time-resolved spectroscopy of the 63 brightest bursts of SGR J1550-5418, detected with the Fermi/Gamma-ray Burst Monitor during its 2008-2009 intense bursting episode. We performed spectral analysis down to 4 ms timescales to characterize the spectral evolution of the bursts. Using a Comptonized model, we find that the peak energy, E-peak, anti-correlates with flux, while the low-energy photon index remains constant at similar to-0.8 up to a flux limit F approximate to 10(-5) erg s(-1) cm(-2). Above this flux value, the E-peak-flux correlation changes sign, and the index positively correlates with the flux reaching similar to 1 at the highest fluxes. Using a two blackbody model, we find that the areas and fluxes of the two emitting regions correlate positively. Further, we study here for the first time the evolution of the temperatures and areas as a function of flux. We find that the area-kT relation follows the lines of constant luminosity at the lowest fluxes, R-2 proportional to kT(-4), with a break at the higher fluxes (F > 10(-5.5) erg s(-1) cm(-2)). The area of the high-kT component increases with the flux while its temperature decreases, which we interpret as being due to an adiabatic cooling process. The area of the low-kT component, on the other hand, appears to saturate at the highest fluxes, toward R-max approximate to 30 km. Assuming that crust quakes are responsible for soft gamma repeater (SGR) bursts and considering Rmax as the maximum radius of the emitting photon-pair plasma fireball, we relate this saturation radius to a minimum excitation radius of the magnetosphere, and we put a lower limit on the internal magnetic field of SGR J1550-5418, B-int greater than or similar to 4.5 Chi 10(15) G.
C1 [Younes, G.] Univ Space Res Assoc, Huntsville, AL 35806 USA.
[Younes, G.; Kouveliotou, C.] NSSTC, Huntsville, AL 35805 USA.
[Kouveliotou, C.; Collazzi, A.] NASA, George C Marshall Space Flight Ctr, Astrophys Off, Huntsville, AL 35812 USA.
[van der Horst, A. J.; Watts, A. L.; Huppenkothen, D.; van der Klis, M.; van Putten, T.; Wijers, R. A. M. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel.
[Bhat, P. N.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
[Gehrels, N.; Mcenery, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gogus, E.; Kaneko, Y.; Lin, L.] Sabanci Univ, TR-34956 Istanbul, Turkey.
[Gruber, D.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Grunblatt, S.] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
RP Younes, G (reprint author), Univ Space Res Assoc, 6767 Old Madison Pike,Suite 450, Huntsville, AL 35806 USA.
OI Wijers, Ralph/0000-0002-3101-1808
FU GBM/Magnetar Key Project (NASA) [NNH07ZDA001-GLAST]; NWO Vidi grant;
European Research Council [247295]
FX This publication is part of the GBM/Magnetar Key Project (NASA grant
NNH07ZDA001-GLAST; PI: C. Kouveliotou). A.L.W. acknowledges support from
an NWO Vidi grant. A.J.v.d.H. and R.A.M.J.W. acknowledge support from
the European Research Council via Advanced Grant No. 247295.
NR 67
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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 APR 10
PY 2014
VL 785
IS 1
AR 52
DI 10.1088/0004-637X/785/1/52
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG8AE
UT WOS:000335639300052
ER
PT J
AU Archambault, S
Aune, T
Behera, B
Beilicke, M
Benbow, W
Berger, K
Bird, R
Biteau, J
Bugaev, V
Byrum, K
Cardenzana, JV
Cerruti, M
Chen, X
Ciupik, L
Connolly, MP
Cui, W
Dumm, J
Errando, M
Falcone, A
Federici, S
Feng, Q
Finley, JP
Fleischhack, H
Fortson, L
Furniss, A
Galante, N
Gillanders, GH
Griffin, S
Griffiths, ST
Grube, J
Gyuk, G
Hanna, D
Holder, J
Hughes, G
Humensky, TB
Johnson, CA
Kaaret, P
Kertzman, M
Khassen, Y
Kieda, D
Krawczynski, H
Krennrich, F
Kumar, S
Lang, MJ
Madhavan, AS
Maier, G
McCann, A
Meagher, K
Moriarty, P
Mukherjee, R
Nieto, D
de Bhroithe, AO
Ong, RA
Otte, AN
Park, N
Pohl, M
Popkow, A
Prokoph, H
Quinn, J
Ragan, K
Rajotte, J
Reyes, LC
Reynolds, PT
Richards, GT
Roache, E
Sembroski, GH
Shahinyan, K
Staszak, D
Telezhinsky, I
Tucci, JV
Tyler, J
Varlotta, A
Vassiliev, VV
Vincent, S
Wakely, SP
Weinstein, A
Welsing, R
Wilhelm, A
Williams, DA
Ackermann, M
Ajello, M
Albert, A
Baldini, L
Bastieri, D
Bellazzini, R
Bissaldi, E
Bregeon, J
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Cavazzuti, E
Charles, E
Chiang, J
Ciprini, S
Claus, R
Cutini, S
D'Ammando, F
de Angelis, A
de Palma, F
Dermer, CD
Digel, SW
Di Venere, L
Drell, PS
Favuzzi, C
Franckowiak, A
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Giordano, F
Giroletti, M
Grenier, IA
Guiriec, S
Jogler, T
Kuss, M
Larsson, S
Latronico, L
Longo, F
Loparco, F
Lubrano, P
Madejski, GM
Mayer, M
Mazziotta, MN
Michelson, PF
Mizuno, T
Monzani, ME
Morselli, A
Murgia, S
Nuss, E
Ohsugi, T
Ormes, JF
Paneque, D
Perkins, JS
Piron, F
Pivato, G
Raino, S
Razzano, M
Reimer, A
Reimer, O
Ritz, S
Schaal, M
Sgro, C
Siskind, EJ
Spinelli, P
Takahashi, H
Tibaldo, L
Tinivella, M
Troja, E
Vianello, G
Werner, M
Wood, M
AF Archambault, S.
Aune, T.
Behera, B.
Beilicke, M.
Benbow, W.
Berger, K.
Bird, R.
Biteau, J.
Bugaev, V.
Byrum, K.
Cardenzana, J. V.
Cerruti, M.
Chen, X.
Ciupik, L.
Connolly, M. P.
Cui, W.
Dumm, J.
Errando, M.
Falcone, A.
Federici, S.
Feng, Q.
Finley, J. P.
Fleischhack, H.
Fortson, L.
Furniss, A.
Galante, N.
Gillanders, G. H.
Griffin, S.
Griffiths, S. T.
Grube, J.
Gyuk, G.
Hanna, D.
Holder, J.
Hughes, G.
Humensky, T. B.
Johnson, C. A.
Kaaret, P.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Kumar, S.
Lang, M. J.
Madhavan, A. S.
Maier, G.
McCann, A.
Meagher, K.
Moriarty, P.
Mukherjee, R.
Nieto, D.
de Bhroithe, A. O'Faolain
Ong, R. A.
Otte, A. N.
Park, N.
Pohl, M.
Popkow, A.
Prokoph, H.
Quinn, J.
Ragan, K.
Rajotte, J.
Reyes, L. C.
Reynolds, P. T.
Richards, G. T.
Roache, E.
Sembroski, G. H.
Shahinyan, K.
Staszak, D.
Telezhinsky, I.
Tucci, J. V.
Tyler, J.
Varlotta, A.
Vassiliev, V. V.
Vincent, S.
Wakely, S. P.
Weinstein, A.
Welsing, R.
Wilhelm, A.
Williams, D. A.
Ackermann, M.
Ajello, M.
Albert, A.
Baldini, L.
Bastieri, D.
Bellazzini, R.
Bissaldi, E.
Bregeon, J.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Cavazzuti, E.
Charles, E.
Chiang, J.
Ciprini, S.
Claus, R.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Dermer, C. D.
Digel, S. W.
Di Venere, L.
Drell, P. S.
Favuzzi, C.
Franckowiak, A.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Giordano, F.
Giroletti, M.
Grenier, I. A.
Guiriec, S.
Jogler, T.
Kuss, M.
Larsson, S.
Latronico, L.
Longo, F.
Loparco, F.
Lubrano, P.
Madejski, G. M.
Mayer, M.
Mazziotta, M. N.
Michelson, P. F.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Murgia, S.
Nuss, E.
Ohsugi, T.
Ormes, J. F.
Paneque, D.
Perkins, J. S.
Piron, F.
Pivato, G.
Raino, S.
Razzano, M.
Reimer, A.
Reimer, O.
Ritz, S.
Schaal, M.
Sgro, C.
Siskind, E. J.
Spinelli, P.
Takahashi, H.
Tibaldo, L.
Tinivella, M.
Troja, E.
Vianello, G.
Werner, M.
Wood, M.
CA VERITAS Collaboration
Fermi LAT Collaboration
TI DEEP BROADBAND OBSERVATIONS OF THE DISTANT GAMMA-RAY BLAZAR PKS 1424+240
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE BL Lacertae objects: individual (PKS 1424+240)-cosmic background
radiation; gamma rays: galaxies
ID EXTRAGALACTIC BACKGROUND LIGHT; SPACE-TELESCOPE MISSION; LARGE-AREA
TELESCOPE; ENERGY COSMIC-RAY; TEV BLAZARS; SPECTRA; REDSHIFT;
ABSORPTION; RADIATION; UNIVERSE
AB We present deep VERITAS observations of the blazar PKS 1424+240, along with contemporaneous Fermi Large Area Telescope, Swift X-ray Telescope, and Swift UV Optical Telescope data between 2009 February 19 and 2013 June 8. This blazar resides at a redshift of z >= 0.6035, displaying a significantly attenuated gamma-ray flux above 100 GeV due to photon absorption via pair-production with the extragalactic background light. We present more than 100 hr of VERITAS observations over three years, a multiwavelength light curve, and the contemporaneous spectral energy distributions. The source shows a higher flux of (2.1 +/- 0.3) x 10(-7) photons m(-2) s(-1) above 120 GeV in 2009 and 2011 as compared to the flux measured in 2013, corresponding to (1.02 +/- 0.08) x 10-7 photons m(-2) s(-1) above 120 GeV. The measured differential very high energy (VHE; E >= 100 GeV) spectral indices are Gamma = 3.8 +/- 0.3, 4.3 +/- 0.6 and 4.5 +/- 0.2 in 2009, 2011, and 2013, respectively. No significant spectral change across the observation epochs is detected. We find no evidence for variability at gamma-ray opacities of greater than tau = 2, where it is postulated that any variability would be small and occur on timescales longer than a year if hadronic cosmic-ray interactions with extragalactic photon fields provide a secondary VHE photon flux. The data cannot rule out such variability due to low statistics.
C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Aune, T.; Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Behera, B.; Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany.
[Beilicke, M.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Cerruti, M.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bird, R.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Biteau, J.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Biteau, J.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Byrum, K.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cardenzana, J. V.; Krennrich, F.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Chen, X.; Federici, S.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Dumm, J.; Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Falcone, A.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Griffiths, S. T.; Kaaret, P.] Stanford Univ, SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Humensky, T. B.; Nieto, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Kertzman, M.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Kieda, D.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[McCann, A.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Moriarty, P.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Moriarty, P.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Park, N.; Wakely, S. P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Reyes, L. C.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Reynolds, P. T.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Furniss, A.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Ackermann, M.; Buehler, R.; Mayer, M.] DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Albert, A.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Franckowiak, A.; Jogler, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Reimer, A.; Reimer, O.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Albert, A.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Franckowiak, A.; Jogler, T.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Reimer, A.; Reimer, O.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Kuss, M.; Razzano, M.; Sgro, C.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bastieri, D.; Buson, S.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bissaldi, E.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Bissaldi, E.] Univ Trieste, I-34127 Trieste, Italy.
[Bregeon, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Rome, Italy.
[D'Ammando, F.; Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Dermer, C. D.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Grenier, I. A.] Univ Paris Diderot, CNRS, CEA IRFU, CEA Saclay,Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Guiriec, S.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Guiriec, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Larsson, S.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Latronico, L.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Longo, F.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Morselli, A.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA.
[Murgia, S.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Ormes, J. F.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Razzano, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Razzano, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.; Werner, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Reimer, A.; Reimer, O.; Werner, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ritz, S.] Natl Acad Sci, Natl Res Council, Res Associate, Washington, DC 20001 USA.
[Schaal, M.; Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Archambault, S (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
EM amy.furniss@gmail.com
RI Reimer, Olaf/A-3117-2013; Bissaldi, Elisabetta/K-7911-2016; Di Venere,
Leonardo/C-7619-2017; Morselli, Aldo/G-6769-2011; Khassen,
Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; Loparco,
Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Gargano,
Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Sgro,
Carmelo/K-3395-2016;
OI Reimer, Olaf/0000-0001-6953-1385; Bissaldi,
Elisabetta/0000-0001-9935-8106; Di Venere, Leonardo/0000-0003-0703-824X;
Cui, Wei/0000-0002-6324-5772; Morselli, Aldo/0000-0002-7704-9553;
Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755;
Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario
/0000-0001-9325-4672; Gargano, Fabio/0000-0002-5055-6395; giglietto,
nicola/0000-0002-9021-2888; Caraveo, Patrizia/0000-0003-2478-8018;
Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864;
Bastieri, Denis/0000-0002-6954-8862; Giroletti,
Marcello/0000-0002-8657-8852; Lang, Mark/0000-0003-4641-4201; Bird,
Ralph/0000-0002-4596-8563; Gasparrini, Dario/0000-0002-5064-9495;
Baldini, Luca/0000-0002-9785-7726
FU U.S. Department of Energy Office of Science; U.S. National Science
Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation
Ireland [SFI 10/RFP/AST2748]; STFC in the UK; NASA through the Space
Telescope Science Institute [HST-GO-12863]; NASA [NAS 5-26555]; INAF in
Italy; CNES in France
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 NSERC in Canada; by Science Foundation
Ireland (SFI 10/RFP/AST2748); and by STFC in the UK. 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.; Support for program
HST-GO-12863 was provided by NASA, awarded through the Space Telescope
Science Institute, operated by the Association of Universities for
Research in Astronomy, Inc., for NASA, under contract NAS 5-26555.; 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.
NR 50
TC 19
Z9 19
U1 1
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2014
VL 785
IS 1
AR L16
DI 10.1088/2041-8205/785/1/L16
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE9RA
UT WOS:000334345000016
ER
PT J
AU Shields, AL
Bitz, CM
Meadows, VS
Joshi, MM
Robinson, TD
AF Shields, Aomawa L.
Bitz, Cecilia M.
Meadows, Victoria S.
Joshi, Manoj M.
Robinson, Tyler D.
TI SPECTRUM-DRIVEN PLANETARY DEGLACIATION DUE TO INCREASES IN STELLAR
LUMINOSITY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrobiology; planetary systems; radiative transfer; stars: low-mass
ID MAIN-SEQUENCE STARS; M-DWARF STARS; SNOWBALL EARTH; HABITABLE ZONE;
ALBEDO FEEDBACK; EVOLUTION; SURFACE; CLIMATE; EXOPLANETS; MODEL
AB Distant planets in globally ice-covered, "nowball," states may depend on increases in their host stars' luminosity to become hospitable for surface life. Using a general circulation model, we simulated the equilibrium climate response of a planet to a range of instellations from an F-, G-, or M-dwarf star. The range of instellation that permits both complete ice cover and at least partially ice-free climate states is a measure of the climate hysteresis that a planet can exhibit. An ice-covered planet with high climate hysteresis would show a higher resistance to the initial loss of surface ice coverage with increases in instellation, and abrupt, extreme ice loss once deglaciation begins. Our simulations indicate that the climate hysteresis depends sensitively on the host star spectral energy distribution. Under fixed CO2 conditions, a planet orbiting an M-dwarf star exhibits a smaller climate hysteresis, requiring smaller instellation to initiate deglaciation than planets orbiting hotter, brighter stars. This is due to the higher absorption of near-infrared radiation by ice on the surfaces and greenhouse gases and clouds in the atmosphere of an M-dwarf planet. Increases in atmospheric CO2 further lower the climate hysteresis, as M-dwarf snowball planets exhibit a larger radiative response than G-dwarf snowball planets for the same increase in CO2. For a smaller hysteresis, planets near the outer edge of the habitable zone will thaw earlier in their evolutionary history, and will experience a less abrupt transition out of global ice cover.
C1 [Shields, Aomawa L.; Meadows, Victoria S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Shields, Aomawa L.; Meadows, Victoria S.] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA.
[Bitz, Cecilia M.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Joshi, Manoj M.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England.
[Robinson, Tyler D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Shields, AL (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA.
EM aomawa@astro.washington.edu
RI Joshi, Manoj/C-1795-2008; Bitz, Cecilia/S-8423-2016;
OI Joshi, Manoj/0000-0002-2948-2811; Bitz, Cecilia/0000-0002-9477-7499;
Robinson, Tyler/0000-0002-3196-414X
FU National Science Foundation [DGE-0718124, DGE-1256082]; National
Aeronautics and Space Administration through the NASA Astrobiology
Institute [NNH05ZDA001C]
FX This material is based upon work supported by the National Science
Foundation Graduate Research Fellowship Program under Grant Nos.
DGE-0718124 and DGE-1256082. This work was performed as part of the NASA
Astrobiology Institute's Virtual Planetary Laboratory Lead Team,
supported by the National Aeronautics and Space Administration through
the NASA Astrobiology Institute under Cooperative Agreement solicitation
NNH05ZDA001C. We thank Dorian Abbot and Raymond Pierrehumbert for
helpful insight on this work, and an anonymous reviewer for extremely
helpful comments that greatly improved the Letter.
NR 41
TC 11
Z9 11
U1 1
U2 18
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2014
VL 785
IS 1
AR L9
DI 10.1088/2041-8205/785/1/L9
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE9RA
UT WOS:000334345000009
ER
PT J
AU Su, Y
Gomory, P
Veronig, A
Temmer, M
Wang, TJ
Vanninathan, K
Gan, WQ
Li, YP
AF Su, Yang
Goemoery, Peter
Veronig, Astrid
Temmer, Manuela
Wang, Tongjiang
Vanninathan, Kamalam
Gan, Weiqun
Li, YouPing
TI SOLAR MAGNETIZED TORNADOES: ROTATIONAL MOTION IN A TORNADO-LIKE
PROMINENCE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: corona; Sun: filaments, prominences; Sun: UV radiation
ID NEUTRAL HYDROGEN; VORTEX FLOWS; FILAMENTS; SPECTROMETER; ABSORPTION;
HELICITY; FEATURES; THREADS; HINODE; FIELDS
AB Su et al. proposed a new explanation for filament formation and eruption, where filament barbs are rotating magnetic structures driven by underlying vortices on the surface. Such structures have been noticed as tornado-like prominences when they appear above the limb. They may play a key role as the source of plasma and twist in filaments. However, no observations have successfully distinguished rotational motion of the magnetic structures in tornado-like prominences from other motions such as oscillation and counter-streaming plasma flows. Here we report evidence of rotational motions in a tornado-like prominence. The spectroscopic observations in two coronal lines were obtained from a specifically designed Hinode/EIS observing program. The data revealed the existence of both cold and million-degree-hot plasma in the prominence leg, supporting the so-called prominence-corona transition region. The opposite velocities at the two sides of the prominence and their persistent time evolution, together with the periodic motions evident in SDO/AIA dark structures, indicate a rotational motion of both cold and hot plasma with a speed of similar to 5 km s(-1).
C1 [Su, Yang; Veronig, Astrid; Temmer, Manuela; Vanninathan, Kamalam] Graz Univ, Inst Phys, IGAM Kanzelhohe Observ, A-8010 Graz, Austria.
[Goemoery, Peter] Slovak Acad Sci, Astron Inst, SK-05960 Tatranska Lomnica, Slovakia.
[Wang, Tongjiang] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wang, Tongjiang] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Gan, Weiqun; Li, YouPing] Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, Nanjing 210008, Jiangsu, Peoples R China.
RP Su, Y (reprint author), Graz Univ, Inst Phys, IGAM Kanzelhohe Observ, Univ Pl 5, A-8010 Graz, Austria.
EM yang.su@uni-graz.at
RI Su, Yang/J-5381-2014; Veronig, Astrid/B-8422-2009;
OI Temmer, Manuela/0000-0003-4867-7558
FU Osterreichischer Austauschdienst (OeAD); Slovak Research and Development
Agency (SRDA) [SK 16/2013, SK-AT-0003-12]; Austrian Science Fund (FWF)
[P24092-N16, V195-N16]; European Community [263086]; Science Grant
Agency [VEGA 2/0108/12]; Slovak Research and Development Agency
[APVV-0816-11]; NASA [NNX12AB34G, NNG11PL10A]
FX The H alpha data was taken by the Solar Magnetic Activity Research
Telescope (SMART) at Hida Observatory, Kyoto University. We downloaded
the data from the SMART T1 Data Archive
(http://www.hida.kyoto-u.ac.jp/SMART/T1.html). SDO is a mission for
NASA's Living With a Star (LWS) Program. This work was supported by the
project of the Osterreichischer Austauschdienst (OeAD) and the Slovak
Research and Development Agency (SRDA) under grant Nos. SK 16/2013 and
SK-AT-0003-12. Y.S., A. V., M. T., and K. V. acknowledge the Austrian
Science Fund (FWF): P24092-N16 and V195-N16. Y.S. and A. V. also
acknowledge the European Community Framework Programme 7, High Energy
Solar Physics Data in Europe (HESPE), grant agreement No.: 263086. P. G.
acknowledges the support from grant VEGA 2/0108/12 of the Science Grant
Agency and from the project of the Slovak Research and Development
Agency under the Contract No. APVV-0816-11. The work of T. W. was
supported by NASA grant NNX12AB34G and the NASA cooperative agreement
NNG11PL10A to CUA. Y.L. and W. G. acknowledge 11233008 from NNSFC and
2011CB811402 from MSTC.
NR 30
TC 14
Z9 14
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2014
VL 785
IS 1
AR L2
DI 10.1088/2041-8205/785/1/L2
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE9RA
UT WOS:000334345000002
ER
PT J
AU Bauschlicher, CW
Ricca, A
AF Bauschlicher, Charles W., Jr.
Ricca, Alessandra
TI Loss of a C2H (n) fragment from pyrene and circumcoronene
SO THEORETICAL CHEMISTRY ACCOUNTS
LA English
DT Article
DE DFT; Polycyclic aromatic hydrocarbon; Loss of C2Hn
ID POLYCYCLIC AROMATIC-HYDROCARBONS; REAXFF; DFTB
AB Reactions at the edge of pyrene and circumcoronene are studied using the B3LYP approach in conjunction with the 4-31G and 6-31G** basis sets. The loss of a C2H (n) fragment from the edge of either molecule requires more than 7 eV, which is much larger than for the loss of an H atom. Some paths can be broken down into a series of less energetic steps, but this does not change the overall endothermicity of the process. The exception is a path where a hydrogen atom adds to pyrene or circumcoronene. The resulting molecule rearranges to have a side group, which is subsequently lost. This process has an overall endothermicity of only about 2.5 eV. This path is actually less endothermic than the loss of an H atom from the same species.
C1 [Bauschlicher, Charles W., Jr.] NASA, Entry Syst & Technol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ricca, Alessandra] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
RP Bauschlicher, CW (reprint author), NASA, Entry Syst & Technol Div, Ames Res Ctr, Mail Stop 230-3, Moffett Field, CA 94035 USA.
EM Charles.W.Bauschlicher@nasa.gov
FU NASA's Astrophysics Theory and Fundamental Physics (ATFP) program
[NNX09AD18G]
FX AR thanks NASA's Astrophysics Theory and Fundamental Physics (ATFP)
(NNX09AD18G) program for its generous support of this work.
NR 15
TC 1
Z9 1
U1 0
U2 5
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1432-881X
EI 1432-2234
J9 THEOR CHEM ACC
JI Theor. Chem. Acc.
PD APR 8
PY 2014
VL 133
IS 5
AR 1479
DI 10.1007/s00214-014-1479-4
PG 5
WC Chemistry, Physical
SC Chemistry
GA AF1BO
UT WOS:000334449600001
ER
PT J
AU Guanter, L
Zhang, YG
Jung, M
Joiner, J
Voigt, M
Berry, JA
Frankenberg, C
Huete, AR
Zarco-Tejada, P
Lee, JE
Moran, MS
Ponce-Campos, G
Beer, C
Camps-Valls, G
Buchmann, N
Gianelle, D
Klumpp, K
Cescatti, A
Baker, JM
Griffis, TJ
AF Guanter, Luis
Zhang, Yongguang
Jung, Martin
Joiner, Joanna
Voigt, Maximilian
Berry, Joseph A.
Frankenberg, Christian
Huete, Alfredo R.
Zarco-Tejada, Pablo
Lee, Jung-Eun
Moran, M. Susan
Ponce-Campos, Guillermo
Beer, Christian
Camps-Valls, Gustavo
Buchmann, Nina
Gianelle, Damiano
Klumpp, Katja
Cescatti, Alessandro
Baker, John M.
Griffis, Timothy J.
TI Global and time-resolved monitoring of crop photosynthesis with
chlorophyll fluorescence
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE crop productivity; carbon fluxes; Earth observation; carbon modeling;
spaceborne spectroscopy
ID SUN-INDUCED FLUORESCENCE; GROSS PRIMARY PRODUCTION; CARBON-DIOXIDE;
CLIMATE; PRODUCTIVITY; SPACE; GOSAT; HEAT; AGRICULTURE; VARIABILITY
AB Photosynthesis is the process by which plants harvest sunlight to produce sugars from carbon dioxide and water. It is the primary source of energy for all life on Earth; hence it is important to understand how this process responds to climate change and human impact. However, model-based estimates of gross primary production (GPP, output from photosynthesis) are highly uncertain, in particular over heavily managed agricultural areas. Recent advances in spectroscopy enable the space-based monitoring of sun-induced chlorophyll fluorescence (SIF) from terrestrial plants. Here we demonstrate that spaceborne SIF retrievals provide a direct measure of the GPP of cropland and grassland ecosystems. Such a strong link with crop photosynthesis is not evident for traditional remotely sensed vegetation indices, nor for more complex carbon cycle models. We use SIF observations to provide a global perspective on agricultural productivity. Our SIF-based crop GPP estimates are 50-75% higher than results from state-of-the-art carbon cycle models over, for example, the US Corn Belt and the Indo-Gangetic Plain, implying that current models severely underestimate the role of management. Our results indicate that SIF data can help us improve our global models for more accurate projections of agricultural productivity and climate impact on crop yields. Extension of our approach to other ecosystems, along with increased observational capabilities for SIF in the near future, holds the prospect of reducing uncertainties in the modeling of the current and future carbon cycle.
C1 [Guanter, Luis; Zhang, Yongguang; Voigt, Maximilian] Free Univ Berlin, Inst Space Sci, D-12165 Berlin, Germany.
[Jung, Martin] Max Planck Inst Biogeochem, Dept Biogeochem Syst, D-07745 Jena, Germany.
[Joiner, Joanna] NASA, Lab Atmospher Chem & Dynam Code 614, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Berry, Joseph A.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Huete, Alfredo R.] Univ Technol Sydney, Plant Funct Biol & Climate Change Cluster, Sydney, NSW 2007, Australia.
[Zarco-Tejada, Pablo] CSIC, Inst Agr Sostenible, Cordoba 14004, Spain.
[Lee, Jung-Eun] Brown Univ, Providence, RI 02912 USA.
[Moran, M. Susan; Ponce-Campos, Guillermo] ARS, USDA, Tucson, AZ 85719 USA.
[Beer, Christian] Stockholm Univ, Dept Appl Environm Sci, S-10691 Stockholm, Sweden.
[Beer, Christian] Stockholm Univ, Bolin Ctr Climate Res, S-10691 Stockholm, Sweden.
[Camps-Valls, Gustavo] Univ Valencia, Image Proc Lab, Valencia 46980, Spain.
[Buchmann, Nina] Eidgenossiche Tech Hsch Zurich, CH-8092 Zurich, Switzerland.
[Gianelle, Damiano] Fdn Edmund Mach, Res & Innovat Ctr, Sustainable Agroecosyst & Bioresources Dept, I-38010 San Michele All Adige, Italy.
[Klumpp, Katja] INRA, Grassland Ecosyst Res Unit, F-63122 Clermont Ferrand, France.
[Cescatti, Alessandro] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-20127 Ispra, Italy.
[Baker, John M.] ARS, USDA, St Paul, MN 55108 USA.
[Griffis, Timothy J.] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA.
RP Guanter, L (reprint author), Free Univ Berlin, Inst Space Sci, D-12165 Berlin, Germany.
EM luis.guanter@wew.fu-berlin.de
RI Griffis, Timothy/A-5707-2011; Joiner, Joanna/D-6264-2012; Beer,
Christian/D-2296-2013; Zarco-Tejada, Pablo J./A-6874-2012; Guanter,
Luis/I-1588-2015; Buchmann, Nina/E-6095-2011; Gianelle,
Damiano/G-9437-2011; Huete, Alfredo/C-1294-2008; Frankenberg,
Christian/A-2944-2013
OI Zhang, Yongguang/0000-0001-8286-300X; Zarco-Tejada, Pablo
J./0000-0003-1433-6165; Guanter, Luis/0000-0002-8389-5764; Gianelle,
Damiano/0000-0001-7697-5793; Huete, Alfredo/0000-0003-2809-2376;
Frankenberg, Christian/0000-0002-0546-5857
FU German Research Foundation; National Aeronautics and Space
Administration (NASA) [NNH10DA001N]; NASA Soil Moisture Active Passive
Science Definition Team [08-SMAPSDT08-0042]; W. M. Keck Foundation
FX We thank T. Meyers (National Oceanic and Atmospheric Administration Air
Resources Laboratory), D. Cook and R. Matamala (Argonne National
Laboratory), A. Suyker ( University of Nebraska), C. Bernhofer
(Technische Universitat Dresden), Z. Nagy (Szent Istvan University), M.
Aubinet (Universite de Liege), W. Kutsch (Johann Heinrich von Thuenen
Institut), and K. Schneider (University of Cologne) for kindly providing
eddy covariance data. We acknowledge C. Monfreda (Arizona State
University), P. H. Verburg (Vrije Universiteit University Amsterdam),
and N. Ramankutty (McGill University) for the crop fraction and NPP data
sets and/or advice on their use, Eumetsat for the GOME-2 data, the
Trendy project for the process-based model runs, and the USDA NASS for
their agricultural inventory data. We also thank the two anonymous
reviewers and Dr. Asner for their valuable suggestions and comments.
MODIS MOD17 GPP data were downloaded from the server of the Numerical
Terradynamic Simulation Group at the University of Montana, MODIS MOD13
data were obtained from the MODIS Land Processes Distributed Active
Archive Center archive, and MERIS-MTCI from the Infoterra Ltd server.
This work used eddy covariance data acquired by AmeriFlux and
GHG-Europe. The work by L. G., Y.Z., and M. V. has been funded by the
Emmy Noether Programme (GlobFluo project) of the German Research
Foundation. J.J. is supported by the National Aeronautics and Space
Administration (NASA) Carbon Cycle Science program (NNH10DA001N) and
G.P.-C. is supported by NASA Soil Moisture Active Passive Science
Definition Team (08-SMAPSDT08-0042). We also thank the W. M. Keck
Foundation for funding the New Methods to Measure Photosynthesis from
Space workshop held at the Caltech Keck Institute for Space Studies.
NR 43
TC 108
Z9 110
U1 19
U2 158
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD APR 8
PY 2014
VL 111
IS 14
BP E1327
EP E1333
DI 10.1073/pnas.1320008111
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AE4VU
UT WOS:000333985200005
PM 24706867
ER
PT J
AU Ruffatto, D
Parness, A
Spenko, M
AF Ruffatto, Donald, III
Parness, Aaron
Spenko, Matthew
TI Improving controllable adhesion on both rough and smooth surfaces with a
hybrid electrostatic/gecko-like adhesive
SO JOURNAL OF THE ROYAL SOCIETY INTERFACE
LA English
DT Article
DE adhesion; electrostatic; gecko; manipulation
ID DIRECTIONAL ADHESION; DRY ADHESIVES; GECKO; ATTACHMENT; ROBOT
AB This paper describes a novel, controllable adhesive that combines the benefits of electrostatic adhesives with gecko-like directional dry adhesives. When working in combination, the two technologies create a positive feedback cycle whose adhesion, depending on the surface type, is often greater than the sum of its parts. The directional dry adhesive brings the electrostatic adhesive closer to the surface, increasing its effect. Similarly, the electrostatic adhesion helps engage more of the directional dry adhesive fibrillar structures, particularly on rough surfaces. This paper presents the new hybrid adhesive's manufacturing process and compares its performance to three other adhesive technologies manufactured using a similar process: reinforced PDMS, electrostatic and directional dry adhesion. Tests were performed on a set of ceramic tiles with varying roughness to quantify its effect on shear adhesive force. The relative effectiveness of the hybrid adhesive increases as the surface roughness is increased. Experimental data are also presented for different substrate materials to demonstrate the enhanced performance achieved with the hybrid adhesive. Results show that the hybrid adhesive provides up to 5.1 x greater adhesion than the electrostatic adhesive or directional dry adhesive technologies alone.
C1 [Ruffatto, Donald, III; Spenko, Matthew] IIT, Dept Mech Engn, Chicago, IL 60616 USA.
[Parness, Aaron] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
RP Ruffatto, D (reprint author), IIT, Dept Mech Engn, Chicago, IL 60616 USA.
EM druffatt@hawk.iit.edu
FU ONR [N00014-10-1-0769]; NASA Office of the Chief Technologist's Space
Technology Research Fellowship
FX This work was supported by ONR grant no. N00014-10-1-0769 and a NASA
Office of the Chief Technologist's Space Technology Research Fellowship.
NR 49
TC 19
Z9 19
U1 5
U2 41
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1742-5689
EI 1742-5662
J9 J R SOC INTERFACE
JI J. R. Soc. Interface
PD APR 6
PY 2014
VL 11
IS 93
AR 20131089
DI 10.1098/rsif.2013.1089
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AC2ZO
UT WOS:000332385000013
PM 24451392
ER
PT J
AU Ma, WP
Jacobs, G
Gao, P
Jermwongratanachai, T
Shafer, WD
Pendyala, VRR
Yen, CH
Klettlinger, JLS
Davis, BH
AF Ma, Wenping
Jacobs, Gary
Gao, Pei
Jermwongratanachai, Thani
Shafer, Wilson D.
Pendyala, Venkat Ramana Rao
Yen, Chia H.
Klettlinger, Jennifer L. S.
Davis, Burtron H.
TI Fischer-Tropsch synthesis: Pore size and Zr promotional effects on the
activity and selectivity of 25%Co/Al2O3 catalysts
SO APPLIED CATALYSIS A-GENERAL
LA English
DT Article
DE Fischer-Tropsch synthesis; Co/Al2O3; Cobalt; Zr; Hydrocarbon
selectivity; XANES; EXAFS
ID IN-SITU EXAFS; CARBON-MONOXIDE HYDROGENATION; ZIRCONIA-MODIFIED ALUMINA;
SUPPORTED COBALT; CO/AL2O3 CATALYSTS; CO HYDROGENATION; REDUCTION;
RHENIUM; REDUCIBILITY; OXIDATION
AB The effects of pore size (10.8 and 25 nm) and zirconium loading (0-5%) on Fischer-Tropsch synthesis (FTS) performance of 25%Co/Al2O3 catalysts were systematically studied at a CO conversion level of similar to 50% under industrially relevant conditions. The catalysts were characterized by adsorption and X-ray spectroscopic techniques in order to understand the relationships between the catalyst physicochemical properties and the FTS performance parameters. Unpromoted wide pore 25%Co/Al2O3 displayed greater stability (CO% rate loss over 150 h of testing: 5.2 versus 27.6%) and 40% higher activity than the narrow pore catalyst. Addition of 1-5% Zr improved the initial activity of the 25%Co/Al2O3 catalysts by 25-71% regardless of support pore size, but the catalyst deactivation rates increased. The activity improvements by Zr for the wide pore and narrow pore catalysts are due to different reasons. XRD, hydrogen-chemisorption, and XANES results suggested that Zr primarily increased Co dispersion for the wide pore catalyst whereas it mainly increased Co reduction for the narrow pore catalysts. The smaller mean Co cluster size observed with the wide pore Co catalyst resulted from a relatively higher fraction of Co residing inside the pores as compared to the narrow pore catalyst.
The unpromoted wide pore catalyst exhibited lower CH4 selectivity (5.9-6.3 versus 8.3-8.9%) and higher C5+ selectivity (88-89.2 versus 80-82%) compared with the narrow pore one. Zr addition decreased CH4 selectivity and increased C5+, selectivity for the narrow pore 25%Co/Al2O3 catalyst, but the opposite trend was observed with the wide pore Co catalyst. Explanations for the selectivity trends (including olefins and CO2) are provided based on the effects of Co size and location, and the resulting changes in H-2/CO mass transport within pores of the Co/Al2O3 catalysts with and without Zr promoter. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Ma, Wenping; Jacobs, Gary; Gao, Pei; Jermwongratanachai, Thani; Shafer, Wilson D.; Pendyala, Venkat Ramana Rao; Davis, Burtron H.] Univ Kentucky, Ctr Appl Energy Res, Lexington, KY 40511 USA.
[Yen, Chia H.; Klettlinger, Jennifer L. S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 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 Jacobs, Gary/M-5349-2015
OI Jacobs, Gary/0000-0003-0691-6717
FU NASA [NNX11AI75A]; Commonwealth of Kentucky
FX The authors thank NASA (Grant No. NNX11AI75A) and the Commonwealth of
Kentucky for financial support for this research project.
NR 43
TC 5
Z9 5
U1 4
U2 58
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 APR 5
PY 2014
VL 475
BP 314
EP 324
DI 10.1016/j.apcata.2014.01.016
PG 11
WC Chemistry, Physical; Environmental Sciences
SC Chemistry; Environmental Sciences & Ecology
GA AG7PP
UT WOS:000335610400039
ER
PT J
AU Brekke, C
Holt, B
Jones, C
Skrunes, S
AF Brekke, Camilla
Holt, Benjamin
Jones, Cathleen
Skrunes, Stine
TI Discrimination of oil spills from newly formed sea ice by synthetic
aperture radar
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Arctic oil spills; Sea ice; Emulsions; SAR; Polarimetry; Mixture
modeling
ID OF-THE-ART; SAR; SCATTERING; PARAMETERS; SATELLITE
AB In this paper we examine the potential of multi-polarization SAR systems to detect and discriminate oil pollution from uncontaminated recently formed thin sea ice in the Arctic Ocean, where both oil and thin sea ice have similar low backscatter returns on SAR imagery. In this study, we present a theoretical model of the relative permittivity of oil-in-sea-ice mixtures and apply it to determine the effect of dielectric properties on the co-polarized backscatter ratio for sea ice, ocean, and oil. To support the theoretical discussion, we invstigate available multi-polarization and multi-frequency SAR measurements. We compare SAR data collected over oil spills in sea-water in the Gulf of Mexico and the North Sea with available similar data covering sea ice in the Arctic region. The results suggest that multi-polarization SAR systems will be useful to detect Arctic oil spills should a spill occur in new and young sea ice conditions, particularly in the marginal ice zones adjacent to the main polar ice pack. (c) 2014 Elsevier Inc. All rights reserved.
C1 [Brekke, Camilla; Skrunes, Stine] UiT Arctic Univ Norway, Dept Phys & Technol, Tromso, Norway.
[Holt, Benjamin; Jones, Cathleen] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Brekke, C (reprint author), UiT Arctic Univ Norway, Dept Phys & Technol, Tromso, Norway.
EM camilla.brekke@uit.no
FU NSC/KSAT; AIRSAR and UAVSAR data are courtesy of NASA/JPL-Caltech; Jet
Propulsion Laboratory, California Institute of Technology
FX The Radarsat-2 data is provided by NSC/KSAT under the NorwegianCanadian
Radarsat agreement 2011. The AIRSAR and UAVSAR data are courtesy of
NASA/JPL-Caltech. This research was carried out in part at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
NR 64
TC 10
Z9 10
U1 2
U2 27
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD APR 5
PY 2014
VL 145
BP 1
EP 14
DI 10.1016/j.rse.2014.01.015
PG 14
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AG0NW
UT WOS:000335113200001
ER
PT J
AU Kuusinen, N
Tomppo, E
Shuai, Y
Berninger, F
AF Kuusinen, Nea
Tomppo, Erkki
Shuai, Yanmin
Berninger, Frank
TI Effects of forest age on albedo in boreal forests estimated from MODIS
and Landsat albedo retrievals
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Albedo; Boreal forest; Forest age; Linear unmixing; MODIS; Landsat
ID BROAD-BAND CONVERSIONS; CONIFEROUS FOREST; SURFACE ALBEDO; BIDIRECTIONAL
REFLECTANCE; THEMATIC MAPPER; BRDF MODELS; NARROW-BAND; IN-SITU; SNOW;
BALANCE
AB The relationship between boreal forest age and albedo in the visible, near-infrared and shortwave broadband was studied using MODIS and Landsat albedo retrievals and forest resource maps. The dependency of forest albedo on stand age was estimated from MODIS albedo retrievals using a linear unmixing approach combined with nonlinear regression. Exponential function was appropriate to describe the decline of coniferous forest albedo with stand age in all seasons and the decline of deciduous broadleaved albedo in winter. The effect of stand age on albedo was stronger for spruce than for pine, and the variation in albedo as a function of stand age was larger in winter than in summer for all species and wavelength regions. When applied to the test data, the albedo values predicted using the estimated age dependent albedo functions produced somewhat better results than when using only the species specific mean albedos as predictors. The tendency of the albedo values predicted using the age dependent functions towards the mean of the observed values suggested that the models did not cover all variation in the species specific forest albedos. A larger variation in the predicted albedos was obtained when age dependent albedo functions were estimated using Landsat albedo estimates. (c) 2014 Elsevier Inc All rights reserved.
C1 [Kuusinen, Nea; Berninger, Frank] Univ Helsinki, Dept Forest Sci, FIN-00014 Helsinki, Finland.
[Tomppo, Erkki] Finnish Forest Res Inst, Vantaa 01301, Finland.
[Shuai, Yanmin] NASA, Goddard Space Flight Ctr, ERT Inc, Greenbelt, MD 20771 USA.
RP Kuusinen, N (reprint author), Univ Helsinki, Dept Forest Sci, POB 27, FIN-00014 Helsinki, Finland.
EM nea.j.kuusinen@helsinki.fi
OI Berninger, Frank/0000-0001-7718-1661
FU Helsinki University Centre for Environment (HENVI); Center of Excellence
in Physics, Chemistry, Biology and Meteorology of Atmospheric
Composition and Climate Change of the Academy of Finland; Nordic Centre
of Excellence: Cryosphere-Atmosphere Interactions in a Changing Arctic
Climate (CRAICC)
FX The study was funded by the Helsinki University Centre for Environment
(HENVI), the Center of Excellence in Physics, Chemistry, Biology and
Meteorology of Atmospheric Composition and Climate Change of the Academy
of Finland and the Nordic Centre of Excellence: Cryosphere-Atmosphere
Interactions in a Changing Arctic Climate (CRAICC). We also thank an
anonymous reviewer for useful suggestions for the manuscript
NR 48
TC 13
Z9 13
U1 2
U2 31
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD APR 5
PY 2014
VL 145
BP 145
EP 153
DI 10.1016/jsse.2014.02.005
PG 9
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AG0NW
UT WOS:000335113200013
ER
PT J
AU Roy, DP
Wulder, MA
Loveland, TR
Woodcock, CE
Allen, RG
Anderson, MC
Helder, D
Irons, JR
Johnson, DM
Kennedy, R
Scambos, T
Schaaf, CB
Schott, JR
Sheng, Y
Vermote, EF
Belward, AS
Bindschadler, R
Cohen, WB
Gao, F
Hipple, JD
Hostert, P
Huntington, J
Justice, CO
Kilic, A
Kovalskyy, V
Lee, ZP
Lymbumer, L
Masek, JG
McCorkel, J
Shuai, Y
Trezza, R
Vogelmann, J
Wynne, RH
Zhu, Z
AF Roy, D. P.
Wulder, M. A.
Loveland, T. R.
Woodcock, C. E.
Allen, R. G.
Anderson, M. C.
Helder, D.
Irons, J. R.
Johnson, D. M.
Kennedy, R.
Scambos, Ta.
Schaaf, C. B.
Schott, J. R.
Sheng, Y.
Vermote, E. F.
Belward, A. S.
Bindschadler, R.
Cohen, W. B.
Gao, F.
Hipple, J. D.
Hostert, P.
Huntington, J.
Justice, C. O.
Kilic, A.
Kovalskyy, V.
Lee, Z. P.
Lymbumer, L.
Masek, J. G.
McCorkel, J.
Shuai, Y.
Trezza, R.
Vogelmann, J.
Wynne, R. H.
Zhu, Z.
TI Landsat-8: Science and product vision for terrestrial global change
research
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Landsat 8; OLI; TIRS; Landsat Science Team
ID CONTERMINOUS UNITED-STATES; DATA CONTINUITY MISSION; TERM ACQUISITION
PLAN; ABSOLUTE RADIOMETRIC CALIBRATION; PLUS ATMOSPHERIC CORRECTION;
GREENLAND ICE-SHEET; FOREST COVER CHANGE; LEAF-AREA INDEX; TIME-SERIES;
LAND-COVER
AB Landsat 8, a NASA and USGS collaboration, acquires global moderate-resolution measurements of the Earth's terrestrial and polar regions in the visible, near-infrared, short wave, and thermal infrared. Landsat 8 extends the remarkable 40 year Landsat record and has enhanced capabilities including new spectral bands in the blue and cirrus cloud-detection portion of the spectrum, two thermal bands, improved sensor signal-to-noise performance and associated improvements in radiometric resolution, and an improved duty cycle that allows collection of a significantly greater number of images per day. This paper introduces the current (2012-2017) Landsat Science Team's efforts to establish an initial understanding of Landsat 8 capabilities and the steps ahead in support of priorities identified by the team. Preliminary evaluation of Landsat 8 capabilities and identification of new science and applications opportunities are described with respect to calibration and radiometric characterization; surface reflectance; surface albedo; surface temperature, evapotranspiration and drought; agriculture; land cover, condition, disturbance and change; fresh and coastal water; and snow and ice. Insights into the development of derived 'higher-lever Landsat products are provided in recognition of the growing need for consistently processed, moderate spatial resolution, large area, long-term terrestrial data records for resource management and for climate and global change studies. The paper concludes with future prospects, emphasizing the opportunities for land imaging constellations by combining Landsat data with data collected from other international sensing systems, and consideration of successor Landsat mission requirements. (c) 2014 The Authors. Published by Elsevier Inc.
C1 [Roy, D. P.; Kovalskyy, V.] S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA.
[Wulder, M. A.] Nat Resources Canada, Pacific Forestry Ctr, Canadian Forest Serv, Victoria, BC V8Z 1M5, Canada.
[Loveland, T. R.; Vogelmann, J.] US Geol Survey, EROS, Sioux Falls, SD 57198 USA.
[Woodcock, C. E.; Kennedy, R.; Zhu, Z.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
[Allen, R. G.; Trezza, R.] Univ Idaho, Res & Extens Ctr, Kimberly, ID 83341 USA.
[Anderson, M. C.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Helder, D.] S Dakota State Univ, Coll Engn, Brookings, SD 57007 USA.
[Irons, J. R.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Johnson, D. M.] USDA, Natl Agr Stat Serv, Fairfax, VA 22030 USA.
[Scambos, Ta.] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80303 USA.
[Schaaf, C. B.; Lee, Z. P.] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA.
[Schott, J. R.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA.
[Sheng, Y.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA.
[Vermote, E. F.] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA.
[Belward, A. S.] European Commiss, Joint Res Ctr, Inst Environm & Sustainabil, I-20133 Milan, Italy.
[Bindschadler, R.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Cohen, W. B.] USDA Forest Serv, Corvallis, OR 97331 USA.
[Gao, F.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Hipple, J. D.] USDA, Risk Management Agcy, Washington, DC 20250 USA.
[Hostert, P.] Humboldt Univ, Dept Geog, D-10099 Berlin, Germany.
[Huntington, J.] Desert Res Inst, Reno, NV 89501 USA.
[Justice, C. O.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Kilic, A.] Univ Nebraska, Sch Nat Resources, Dept Civil Engn, Lincoln, NE 68516 USA.
[Lymbumer, L.] Geosci Australia, Canberra, ACT 2601, Australia.
[Masek, J. G.; McCorkel, J.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Shuai, Y.] NASAs, Goddard Space Flight Ctr, ERT Inc, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Wynne, R. H.] Virginia Tech, Forest Resources & Environm Conservat, Blacksburg, VA 24061 USA.
RP Roy, DP (reprint author), S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA.
RI Masek, Jeffrey/D-7673-2012; Anderson, Martha/C-1720-2015; McCorkel,
Joel/D-4454-2012; Zhu, Zhe/K-3518-2015; Wulder, Michael/J-5597-2016;
OI Anderson, Martha/0000-0003-0748-5525; McCorkel,
Joel/0000-0003-2853-2036; Zhu, Zhe/0000-0001-8283-6407; Wulder,
Michael/0000-0002-6942-1896; Vogelmann, James/0000-0002-0804-5823
FU USGS-NASA Landsat Science Team
FX We are grateful to the NASA-USGS-industry Landsat Data Continuity
Mission (LDCM) development team for their efforts to meet an aggressive
launch schedule, and we thank the USGS Climate and Land Use Change
Mission's Land Remote Sensing Program and the Earth Resources
Observation and Science (EROS) Center for co-sponsoring and funding the
USGS-NASA Landsat Science Team.
NR 194
TC 249
Z9 259
U1 37
U2 225
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD APR 5
PY 2014
VL 145
BP 154
EP 172
DI 10.1016/j.rse.2014.02.001
PG 19
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA AG0NW
UT WOS:000335113200014
ER
PT J
AU Aasi, J
Abadie, J
Abbott, BP
Abbott, R
Abbott, T
Abernathy, MR
Accadia, T
Acernese, F
Adams, C
Adams, T
Adhikari, RX
Affeldt, C
Agathos, M
Aggarwal, N
Aguiar, OD
Ajith, P
Allen, B
Allocca, A
Ceron, EA
Amariutei, D
Anderson, RA
Anderson, SB
Anderson, WG
Arai, K
Araya, MC
Arceneaux, C
Areeda, J
Ast, S
Aston, SM
Astone, P
Aufmuth, P
Aulbert, C
Austin, L
Aylott, BE
Babak, S
Baker, PT
Ballardin, G
Ballmer, SW
Barayoga, JC
Barker, D
Barnum, SH
Barone, F
Barr, B
Barsotti, L
Barsuglia, M
Barton, MA
Bartos, I
Bassiri, R
Basti, A
Batch, J
Bauchrowitz, J
Bauer, TS
Bebronne, M
Behnke, B
Bejger, M
Beker, MG
Bell, AS
Bell, C
Belopolski, I
Bergmann, G
Berliner, JM
Bersanetti, D
Bertolini, A
Bessis, D
Betzwieser, J
Beyersdorf, PT
Bhadbhade, T
Bilenko, IA
Billingsley, G
Birch, J
Bitossi, M
Bizouard, MA
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Blom, M
Bock, O
Bodiya, TP
Boer, M
Bogan, C
Bond, C
Bondu, F
Bonelli, L
Bonnand, R
Bork, R
Born, M
Boschi, V
Bose, S
Bosi, L
Bowers, J
Bradaschia, C
Brady, PR
Braginsky, VB
Branchesi, M
Brannen, CA
Brau, JE
Breyer, J
Briant, T
Bridges, DO
Brillet, A
Brinkmann, M
Brisson, V
Britzger, M
Brooks, AF
Brown, DA
Brown, DD
Bruckner, F
Bulik, T
Bulten, HJ
Buonanno, A
Buskulic, D
Buy, C
Byer, RL
Cadonati, L
Cagnoli, G
Bustillo, JC
Calloni, E
Camp, JB
Campsie, P
Cannon, KC
Canuel, B
Cao, J
Capano, CD
Carbognani, F
Carbone, L
Caride, S
Castiglia, A
Caudill, S
Cavaglia, M
Cavalier, F
Cavalieri, R
Cella, G
Cepeda, C
Cesarini, E
Chakraborty, R
Chalermsongsak, T
Chao, S
Charlton, P
Chassande-Mottin, E
Chen, X
Chen, Y
Chincarini, A
Chiummo, A
Cho, HS
Chow, J
Christensen, N
Chu, Q
Chua, SSY
Chung, S
Ciani, G
Clara, F
Clark, DE
Clark, JA
Cleva, F
Coccia, E
Cohadon, PF
Colla, A
Colombini, M
Constancio, M
Conte, A
Conte, R
Cook, D
Corbitt, TR
Cordier, M
Cornish, N
Corsi, A
Costa, CA
Coughlin, MW
Coulon, JP
Countryman, S
Couvares, P
Coward, DM
Cowart, M
Coyne, DC
Craig, K
Creighton, JDE
Creighton, TD
Crowder, SG
Cumming, A
Cunningham, L
Cuoco, E
Dahl, K
Dal Canton, T
Damjanic, M
Danilishin, SL
D'Antonio, S
Danzmann, K
Dattilo, V
Daudert, B
Daveloza, H
Davier, M
Davies, GS
Daw, EJ
Day, R
Dayanga, T
De Rosa, R
Debreczeni, G
Degallaix, J
Del Pozzo, W
Deleeuw, E
Deleglise, S
Denker, T
Dent, T
Dereli, H
Dergachev, V
DeRosa, R
DeSalvo, R
Dhurandhar, S
Di Fiore, L
Di Lieto, A
Di Palma, I
Di Virgilio, A
Diaz, M
Dietz, A
Dmitry, K
Donovan, F
Dooley, KL
Doravari, S
Drago, M
Drever, RWP
Driggers, JC
Du, Z
Dumas, JC
Dwyer, S
Eberle, T
Edwards, M
Effler, A
Ehrens, P
Eichholz, J
Eikenberry, SS
Endroczi, G
Essick, R
Etzel, T
Evans, K
Evans, M
Evans, T
Factourovich, M
Fafone, V
Fairhurst, S
Fang, Q
Farinon, S
Farr, B
Farr, W
Favata, M
Fazi, D
Fehrmann, H
Feldbaum, D
Ferrante, I
Ferrini, F
Fidecaro, F
Finn, LS
Fiori, I
Fisher, R
Flaminio, R
Foley, E
Foley, S
Forsi, E
Fotopoulos, N
Fournier, JD
Franco, S
Frasca, S
Frasconi, F
Frede, M
Frei, M
Frei, Z
Freise, A
Frey, R
Fricke, TT
Fritschel, P
Frolov, VV
Fujimoto, MK
Fulda, P
Fyffe, M
Gair, J
Gammaitoni, L
Garcia, J
Garufi, F
Gehrels, N
Gemme, G
Genin, E
Gennai, A
Gergely, L
Ghosh, S
Giaime, JA
Giampanis, S
Giardina, KD
Giazotto, A
Gil-Casanova, S
Gill, C
Gleason, J
Goetz, E
Goetz, R
Gondan, L
Gonzalez, G
Gordon, N
Gorodetsky, ML
Gossan, S
Gossler, S
Gouaty, R
Graef, C
Graff, PB
Granata, M
Grant, A
Gras, S
Gray, C
Greenhalgh, RJS
Gretarsson, AM
Griffo, C
Groot, P
Grote, H
Grover, K
Grunewald, S
Guidi, GM
Guido, C
Gushwa, KE
Gustafson, EK
Gustafson, R
Hall, B
Hall, E
Hammer, D
Hammond, G
Hanke, M
Hanks, J
Hanna, C
Hanson, J
Harms, J
Harry, GM
Harry, IW
Harstad, ED
Hartman, MT
Haughian, K
Hayama, K
Heefner, J
Heidmann, A
Heintze, M
Heitmann, H
Hello, P
Hemming, G
Hendry, M
Heng, IS
Heptonstall, AW
Heurs, M
Hild, S
Hoak, D
Hodge, KA
Holt, K
Holtrop, M
Hong, T
Hooper, S
Horrom, T
Hosken, DJ
Hough, J
Howell, EJ
Hu, Y
Hua, Z
Huang, V
Huerta, EA
Hughey, B
Husa, S
Huttner, SH
Huynh, M
Huynh-Dinh, T
Iafrate, J
Ingram, DR
Inta, R
Isogai, T
Ivanov, A
Iyer, BR
Izumi, K
Jacobson, M
James, E
Jang, H
Jang, YJ
Jaranowski, P
Jimenez-Forteza, F
Johnson, WW
Jones, D
Jones, DI
Jones, R
Jonker, RJG
Ju, L
Haris, K
Kalmus, P
Kalogera, V
Kandhasamy, S
Kang, G
Kanner, JB
Kasprzack, M
Kasturi, R
Katsavounidis, E
Katzman, W
Kaufer, H
Kaufman, K
Kawabe, K
Kawamura, S
Kawazoe, F
Kefelian, F
Keitel, D
Kelley, DB
Kells, W
Keppel, DG
Khalaidovski, A
Khalili, FY
Khazanov, EA
Kim, BK
Kim, C
Kim, K
Kim, N
Kim, W
Kim, YM
King, EJ
King, PJ
Kinzel, DL
Kissel, JS
Klimenko, S
Kline, J
Koehlenbeck, S
Kokeyama, K
Kondrashov, V
Koranda, S
Korth, WZ
Kowalska, I
Kozak, D
Kremin, A
Kringel, V
Krolak, A
Kucharczyk, C
Kudla, S
Kuehn, G
Kumar, A
Kumar, P
Kumar, R
Kurdyumov, R
Kwee, P
Landry, M
Lantz, B
Larson, S
Lasky, PD
Lawrie, C
Lazzarini, A
Le Roux, A
Leaci, P
Lebigot, EO
Lee, CH
Lee, HK
Lee, HM
Lee, J
Lee, J
Leonardi, M
Leong, JR
Leroy, N
Letendre, N
Levine, B
Lewis, JB
Lhuillier, V
Li, TGF
Lin, AC
Littenberg, TB
Litvine, V
Liu, F
Liu, H
Liu, Y
Liu, Z
Lloyd, D
Lockerbie, NA
Lockett, V
Lodhia, D
Loew, K
Logue, J
Lombardi, AL
Lorenzini, M
Loriette, V
Lormand, M
Losurdo, G
Lough, J
Luan, J
Lubinski, MJ
Luck, H
Lundgren, AP
Macarthur, J
Macdonald, E
Machenschalk, B
MacInnis, M
Macleod, DM
Magana-Sandoval, F
Mageswaran, M
Mailand, K
Majorana, E
Maksimovic, I
Malvezzi, V
Man, N
Manca, GM
Mandel, I
Mandic, V
Mangano, V
Mantovani, M
Marchesoni, F
Marion, F
Marka, S
Marka, Z
Markosyan, A
Maros, E
Marque, J
Martelli, F
Martin, IW
Martin, RM
Martinelli, L
Martynov, D
Marx, JN
Mason, K
Masserot, A
Massinger, TJ
Matichard, F
Matone, L
Matzner, RA
Mavalvala, N
May, G
Mazumder, N
Mazzolo, G
McCarthy, R
McClelland, DE
McGuire, SC
McIntyre, G
McIver, J
Meacher, D
Meadors, GD
Mehmet, M
Meidam, J
Meier, T
Melatos, A
Mendell, G
Mercer, RA
Meshkov, S
Messenger, C
Meyer, MS
Miao, H
Michel, C
Mikhailov, EE
Milano, L
Miller, J
Minenkov, Y
Mingarelli, CMF
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Moe, B
Mohan, M
Mohapatra, SRP
Mokler, F
Moraru, D
Moreno, G
Morgado, N
Mori, T
Morriss, SR
Mossavi, K
Mours, B
Mow-Lowry, CM
Mueller, CL
Mueller, G
Mukherjee, S
Mullavey, A
Munch, J
Murphy, D
Murray, PG
Mytidis, A
Nagy, MF
Kumar, DN
Nardecchia, I
Nash, T
Naticchioni, L
Nayak, R
Necula, V
Nelemans, G
Neri, I
Neri, M
Newton, G
Nguyen, T
Nishida, E
Nishizawa, A
Nitz, A
Nocera, F
Nolting, D
Normandin, ME
Nuttall, LK
Ochsner, E
O'Dell, J
Oelker, E
Ogin, GH
Oh, JJ
Oh, SH
Ohme, F
Oppermann, P
O'Reilly, B
Larcher, WO
O'Shaughnessy, R
Osthelder, C
Ott, CD
Ottaway, DJ
Ottens, RS
Ou, J
Overmier, H
Owen, BJ
Padilla, C
Pai, A
Palomba, C
Pan, Y
Pankow, C
Paoletti, F
Paoletti, R
Papa, MA
Paris, H
Pasqualetti, A
Passaquieti, R
Passuello, D
Pedraza, M
Peiris, P
Penn, S
Perreca, A
Phelps, M
Pichot, M
Pickenpack, M
Piergiovanni, F
Pierro, V
Pinard, L
Pindor, B
Pinto, IM
Pitkin, M
Poeld, J
Poggiani, R
Poole, V
Poux, C
Predoi, V
Prestegard, T
Price, LR
Prijatelj, M
Principe, M
Privitera, S
Prix, R
Prodi, GA
Prokhorov, L
Puncken, O
Punturo, M
Puppo, P
Quetschke, V
Quintero, E
Quitzow-James, R
Raab, FJ
Rabeling, DS
Racz, I
Radkins, H
Raffai, P
Raja, S
Rajalakshmi, G
Rakhmanov, M
Ramet, C
Rapagnani, P
Raymond, V
Re, V
Reed, CM
Reed, T
Regimbau, T
Reid, S
Reitze, DH
Ricci, F
Riesen, R
Riles, K
Robertson, NA
Robinet, F
Rocchi, A
Roddy, S
Rodriguez, C
Rodruck, M
Roever, C
Rolland, L
Rollins, JG
Romano, R
Romanov, G
Romie, JH
Rosinska, D
Rowan, S
Rudger, A
Ruggi, P
Ryan, K
Salemi, F
Sammut, L
Sandberg, V
Sanders, J
Sannibale, V
Santiago-Prieto, I
Saracco, E
Sassolas, B
Sathyaprakash, BS
Saulson, PR
Savage, R
Schilling, R
Schnabel, R
Schofield, RMS
Schreiber, E
Schuette, D
Schulz, B
Schutz, BF
Schwinberg, P
Scott, J
Scott, SM
Seifert, F
Sellers, D
Sengupta, AS
Sentenac, D
Sergeev, A
Shaddock, D
Shah, S
Shahriar, MS
Shaltev, M
Shapiro, B
Shawhan, P
Shoemaker, DH
Sidery, TL
Siellez, K
Siemens, X
Sigg, D
Simakov, D
Singer, A
Singer, L
Sintes, AM
Skelton, GR
Slagmolen, BJJ
Slutsky, J
Smith, JR
Smith, MR
Smith, RJE
Smith-Lefebvre, ND
Soden, K
Son, EJ
Sorazu, B
Souradeep, T
Sperandio, L
Staley, A
Steinert, E
Steinlechner, J
Steinlechner, S
Steplewski, S
Stevens, D
Stochino, A
Stone, R
Strain, KA
Straniero, N
Strigin, S
Stroeer, AS
Sturani, R
Stuver, AL
Summerscales, TZ
Susmithan, S
Sutton, PJ
Swinkels, B
Szeifert, G
Tacca, M
Talukder, D
Tang, L
Tanner, DB
Tarabrin, SP
Taylor, R
ter Braack, APM
Thirugnanasambandam, MP
Thomas, M
Thomas, P
Thorne, KA
Thorne, KS
Thrane, E
Tiwari, V
Tokmakov, KV
Tomlinson, C
Toncelli, A
Tonelli, M
Torre, O
Torres, CV
Torrie, CI
Travasso, F
Traylor, G
Tse, M
Ugolini, D
Unnikrishnan, CS
Vahlbruch, H
Vajente, G
Vallisneri, M
Van den Brand, JFJ
Van den Broeck, C
van der Putten, S
van der Sluys, MV
van Heijningen, J
van Veggel, AA
Vass, S
Vasuth, M
Vaulin, R
Vecchio, A
Vedovato, G
Veitch, J
Veitch, PJ
Venkateswara, K
Verkindt, D
Vetrano, F
Vicere, A
Vincent-Finley, R
Vinet, JY
Vitale, S
Vlcek, B
Vo, T
Vocca, H
Vorvick, C
Vousden, WD
Vrinceanu, D
Vyachanin, SP
Wade, A
Wade, L
Wade, M
Waldman, SJ
Walker, M
Wallace, L
Wan, Y
Wang, J
Wang, M
Wang, X
Wanner, A
Ward, RL
Was, M
Weaver, B
Wei, LW
Weinert, M
Weinstein, AJ
Weiss, R
Welborn, T
Wen, L
Wessels, P
West, M
Westphal, T
Wette, K
Whelan, JT
Whitcomb, SE
White, DJ
Whiting, BF
Wibowo, S
Wiesner, K
Wilkinson, C
Williams, L
Williams, R
Williams, T
Willis, JL
Willke, B
Wimmer, M
Winkelmann, L
Winkler, W
Wipf, CC
Wittel, H
Woan, G
Worden, J
Yablon, J
Yakushin, I
Yamamoto, H
Yancey, CC
Yang, H
Yeaton-Massey, D
Yoshida, S
Yum, H
Yvert, M
Zadrozny, A
Zanolin, M
Zendri, JP
Zhang, F
Zhang, L
Zhao, C
Zhu, H
Zhu, XJ
Zotov, N
Zucker, ME
Zweizig, J
AF Aasi, J.
Abadie, J.
Abbott, B. P.
Abbott, R.
Abbott, T.
Abernathy, M. R.
Accadia, T.
Acernese, F.
Adams, C.
Adams, T.
Adhikari, R. X.
Affeldt, C.
Agathos, M.
Aggarwal, N.
Aguiar, O. D.
Ajith, P.
Allen, B.
Allocca, A.
Ceron, E. Amador
Amariutei, D.
Anderson, R. A.
Anderson, S. B.
Anderson, W. G.
Arai, K.
Araya, M. C.
Arceneaux, C.
Areeda, J.
Ast, S.
Aston, S. M.
Astone, P.
Aufmuth, P.
Aulbert, C.
Austin, L.
Aylott, B. E.
Babak, S.
Baker, P. T.
Ballardin, G.
Ballmer, S. W.
Barayoga, J. C.
Barker, D.
Barnum, S. H.
Barone, F.
Barr, B.
Barsotti, L.
Barsuglia, M.
Barton, M. A.
Bartos, I.
Bassiri, R.
Basti, A.
Batch, J.
Bauchrowitz, J.
Bauer, Th. S.
Bebronne, M.
Behnke, B.
Bejger, M.
Beker, M. G.
Bell, A. S.
Bell, C.
Belopolski, I.
Bergmann, G.
Berliner, J. M.
Bersanetti, D.
Bertolini, A.
Bessis, D.
Betzwieser, J.
Beyersdorf, P. T.
Bhadbhade, T.
Bilenko, I. A.
Billingsley, G.
Birch, J.
Bitossi, M.
Bizouard, M. A.
Black, E.
Blackburn, J. K.
Blackburn, L.
Blair, D.
Blom, M.
Bock, O.
Bodiya, T. P.
Boer, M.
Bogan, C.
Bond, C.
Bondu, F.
Bonelli, L.
Bonnand, R.
Bork, R.
Born, M.
Boschi, V.
Bose, S.
Bosi, L.
Bowers, J.
Bradaschia, C.
Brady, P. R.
Braginsky, V. B.
Branchesi, M.
Brannen, C. A.
Brau, J. E.
Breyer, J.
Briant, T.
Bridges, D. O.
Brillet, A.
Brinkmann, M.
Brisson, V.
Britzger, M.
Brooks, A. F.
Brown, D. A.
Brown, D. D.
Brueckner, F.
Bulik, T.
Bulten, H. J.
Buonanno, A.
Buskulic, D.
Buy, C.
Byer, R. L.
Cadonati, L.
Cagnoli, G.
Calderon Bustillo, J.
Calloni, E.
Camp, J. B.
Campsie, P.
Cannon, K. C.
Canuel, B.
Cao, J.
Capano, C. D.
Carbognani, F.
Carbone, L.
Caride, S.
Castiglia, A.
Caudill, S.
Cavaglia, M.
Cavalier, F.
Cavalieri, R.
Cella, G.
Cepeda, C.
Cesarini, E.
Chakraborty, R.
Chalermsongsak, T.
Chao, S.
Charlton, P.
Chassande-Mottin, E.
Chen, X.
Chen, Y.
Chincarini, A.
Chiummo, A.
Cho, H. S.
Chow, J.
Christensen, N.
Chu, Q.
Chua, S. S. Y.
Chung, S.
Ciani, G.
Clara, F.
Clark, D. E.
Clark, J. A.
Cleva, F.
Coccia, E.
Cohadon, P. -F.
Colla, A.
Colombini, M.
Constancio, M., Jr.
Conte, A.
Conte, R.
Cook, D.
Corbitt, T. R.
Cordier, M.
Cornish, N.
Corsi, A.
Costa, C. A.
Coughlin, M. W.
Coulon, J. -P.
Countryman, S.
Couvares, P.
Coward, D. M.
Cowart, M.
Coyne, D. C.
Craig, K.
Creighton, J. D. E.
Creighton, T. D.
Crowder, S. G.
Cumming, A.
Cunningham, L.
Cuoco, E.
Dahl, K.
Dal Canton, T.
Damjanic, M.
Danilishin, S. L.
D'Antonio, S.
Danzmann, K.
Dattilo, V.
Daudert, B.
Daveloza, H.
Davier, M.
Davies, G. S.
Daw, E. J.
Day, R.
Dayanga, T.
De Rosa, R.
Debreczeni, G.
Degallaix, J.
Del Pozzo, W.
Deleeuw, E.
Deleglise, S.
Denker, T.
Dent, T.
Dereli, H.
Dergachev, V.
DeRosa, R.
DeSalvo, R.
Dhurandhar, S.
Di Fiore, L.
Di Lieto, A.
Di Palma, I.
Di Virgilio, A.
Diaz, M.
Dietz, A.
Dmitry, K.
Donovan, F.
Dooley, K. L.
Doravari, S.
Drago, M.
Drever, R. W. P.
Driggers, J. C.
Du, Z.
Dumas, J. -C.
Dwyer, S.
Eberle, T.
Edwards, M.
Effler, A.
Ehrens, P.
Eichholz, J.
Eikenberry, S. S.
Endroczi, G.
Essick, R.
Etzel, T.
Evans, K.
Evans, M.
Evans, T.
Factourovich, M.
Fafone, V.
Fairhurst, S.
Fang, Q.
Farinon, S.
Farr, B.
Farr, W.
Favata, M.
Fazi, D.
Fehrmann, H.
Feldbaum, D.
Ferrante, I.
Ferrini, F.
Fidecaro, F.
Finn, L. S.
Fiori, I.
Fisher, R.
Flaminio, R.
Foley, E.
Foley, S.
Forsi, E.
Fotopoulos, N.
Fournier, J. -D.
Franco, S.
Frasca, S.
Frasconi, F.
Frede, M.
Frei, M.
Frei, Z.
Freise, A.
Frey, R.
Fricke, T. T.
Fritschel, P.
Frolov, V. V.
Fujimoto, M. -K.
Fulda, P.
Fyffe, M.
Gair, J.
Gammaitoni, L.
Garcia, J.
Garufi, F.
Gehrels, N.
Gemme, G.
Genin, E.
Gennai, A.
Gergely, L.
Ghosh, S.
Giaime, J. A.
Giampanis, S.
Giardina, K. D.
Giazotto, A.
Gil-Casanova, S.
Gill, C.
Gleason, J.
Goetz, E.
Goetz, R.
Gondan, L.
Gonzalez, G.
Gordon, N.
Gorodetsky, M. L.
Gossan, S.
Gossler, S.
Gouaty, R.
Graef, C.
Graff, P. B.
Granata, M.
Grant, A.
Gras, S.
Gray, C.
Greenhalgh, R. J. S.
Gretarsson, A. M.
Griffo, C.
Groot, P.
Grote, H.
Grover, K.
Grunewald, S.
Guidi, G. M.
Guido, C.
Gushwa, K. E.
Gustafson, E. K.
Gustafson, R.
Hall, B.
Hall, E.
Hammer, D.
Hammond, G.
Hanke, M.
Hanks, J.
Hanna, C.
Hanson, J.
Harms, J.
Harry, G. M.
Harry, I. W.
Harstad, E. D.
Hartman, M. T.
Haughian, K.
Hayama, K.
Heefner, J.
Heidmann, A.
Heintze, M.
Heitmann, H.
Hello, P.
Hemming, G.
Hendry, M.
Heng, I. S.
Heptonstall, A. W.
Heurs, M.
Hild, S.
Hoak, D.
Hodge, K. A.
Holt, K.
Holtrop, M.
Hong, T.
Hooper, S.
Horrom, T.
Hosken, D. J.
Hough, J.
Howell, E. J.
Hu, Y.
Hua, Z.
Huang, V.
Huerta, E. A.
Hughey, B.
Husa, S.
Huttner, S. H.
Huynh, M.
Huynh-Dinh, T.
Iafrate, J.
Ingram, D. R.
Inta, R.
Isogai, T.
Ivanov, A.
Iyer, B. R.
Izumi, K.
Jacobson, M.
James, E.
Jang, H.
Jang, Y. J.
Jaranowski, P.
Jimenez-Forteza, F.
Johnson, W. W.
Jones, D.
Jones, D. I.
Jones, R.
Jonker, R. J. G.
Ju, L.
Haris, K.
Kalmus, P.
Kalogera, V.
Kandhasamy, S.
Kang, G.
Kanner, J. B.
Kasprzack, M.
Kasturi, R.
Katsavounidis, E.
Katzman, W.
Kaufer, H.
Kaufman, K.
Kawabe, K.
Kawamura, S.
Kawazoe, F.
Kefelian, F.
Keitel, D.
Kelley, D. B.
Kells, W.
Keppel, D. G.
Khalaidovski, A.
Khalili, F. Y.
Khazanov, E. A.
Kim, B. K.
Kim, C.
Kim, K.
Kim, N.
Kim, W.
Kim, Y. -M.
King, E. J.
King, P. J.
Kinzel, D. L.
Kissel, J. S.
Klimenko, S.
Kline, J.
Koehlenbeck, S.
Kokeyama, K.
Kondrashov, V.
Koranda, S.
Korth, W. Z.
Kowalska, I.
Kozak, D.
Kremin, A.
Kringel, V.
Krolak, A.
Kucharczyk, C.
Kudla, S.
Kuehn, G.
Kumar, A.
Kumar, P.
Kumar, R.
Kurdyumov, R.
Kwee, P.
Landry, M.
Lantz, B.
Larson, S.
Lasky, P. D.
Lawrie, C.
Lazzarini, A.
Le Roux, A.
Leaci, P.
Lebigot, E. O.
Lee, C. -H.
Lee, H. K.
Lee, H. M.
Lee, J.
Lee, J.
Leonardi, M.
Leong, J. R.
Leroy, N.
Letendre, N.
Levine, B.
Lewis, J. B.
Lhuillier, V.
Li, T. G. F.
Lin, A. C.
Littenberg, T. B.
Litvine, V.
Liu, F.
Liu, H.
Liu, Y.
Liu, Z.
Lloyd, D.
Lockerbie, N. A.
Lockett, V.
Lodhia, D.
Loew, K.
Logue, J.
Lombardi, A. L.
Lorenzini, M.
Loriette, V.
Lormand, M.
Losurdo, G.
Lough, J.
Luan, J.
Lubinski, M. J.
Lueck, H.
Lundgren, A. P.
Macarthur, J.
Macdonald, E.
Machenschalk, B.
MacInnis, M.
Macleod, D. M.
Magana-Sandoval, F.
Mageswaran, M.
Mailand, K.
Majorana, E.
Maksimovic, I.
Malvezzi, V.
Man, N.
Manca, G. M.
Mandel, I.
Mandic, V.
Mangano, V.
Mantovani, M.
Marchesoni, F.
Marion, F.
Marka, S.
Marka, Z.
Markosyan, A.
Maros, E.
Marque, J.
Martelli, F.
Martin, I. W.
Martin, R. M.
Martinelli, L.
Martynov, D.
Marx, J. N.
Mason, K.
Masserot, A.
Massinger, T. J.
Matichard, F.
Matone, L.
Matzner, R. A.
Mavalvala, N.
May, G.
Mazumder, N.
Mazzolo, G.
McCarthy, R.
McClelland, D. E.
McGuire, S. C.
McIntyre, G.
McIver, J.
Meacher, D.
Meadors, G. D.
Mehmet, M.
Meidam, J.
Meier, T.
Melatos, A.
Mendell, G.
Mercer, R. A.
Meshkov, S.
Messenger, C.
Meyer, M. S.
Miao, H.
Michel, C.
Mikhailov, E. E.
Milano, L.
Miller, J.
Minenkov, Y.
Mingarelli, C. M. F.
Mitra, S.
Mitrofanov, V. P.
Mitselmakher, G.
Mittleman, R.
Moe, B.
Mohan, M.
Mohapatra, S. R. P.
Mokler, F.
Moraru, D.
Moreno, G.
Morgado, N.
Mori, T.
Morriss, S. R.
Mossavi, K.
Mours, B.
Mow-Lowry, C. M.
Mueller, C. L.
Mueller, G.
Mukherjee, S.
Mullavey, A.
Munch, J.
Murphy, D.
Murray, P. G.
Mytidis, A.
Nagy, M. F.
Kumar, D. Nanda
Nardecchia, I.
Nash, T.
Naticchioni, L.
Nayak, R.
Necula, V.
Nelemans, G.
Neri, I.
Neri, M.
Newton, G.
Nguyen, T.
Nishida, E.
Nishizawa, A.
Nitz, A.
Nocera, F.
Nolting, D.
Normandin, M. E.
Nuttall, L. K.
Ochsner, E.
O'Dell, J.
Oelker, E.
Ogin, G. H.
Oh, J. J.
Oh, S. H.
Ohme, F.
Oppermann, P.
O'Reilly, B.
Larcher, W. Ortega
O'Shaughnessy, R.
Osthelder, C.
Ott, C. D.
Ottaway, D. J.
Ottens, R. S.
Ou, J.
Overmier, H.
Owen, B. J.
Padilla, C.
Pai, A.
Palomba, C.
Pan, Y.
Pankow, C.
Paoletti, F.
Paoletti, R.
Papa, M. A.
Paris, H.
Pasqualetti, A.
Passaquieti, R.
Passuello, D.
Pedraza, M.
Peiris, P.
Penn, S.
Perreca, A.
Phelps, M.
Pichot, M.
Pickenpack, M.
Piergiovanni, F.
Pierro, V.
Pinard, L.
Pindor, B.
Pinto, I. M.
Pitkin, M.
Poeld, J.
Poggiani, R.
Poole, V.
Poux, C.
Predoi, V.
Prestegard, T.
Price, L. R.
Prijatelj, M.
Principe, M.
Privitera, S.
Prix, R.
Prodi, G. A.
Prokhorov, L.
Puncken, O.
Punturo, M.
Puppo, P.
Quetschke, V.
Quintero, E.
Quitzow-James, R.
Raab, F. J.
Rabeling, D. S.
Racz, I.
Radkins, H.
Raffai, P.
Raja, S.
Rajalakshmi, G.
Rakhmanov, M.
Ramet, C.
Rapagnani, P.
Raymond, V.
Re, V.
Reed, C. M.
Reed, T.
Regimbau, T.
Reid, S.
Reitze, D. H.
Ricci, F.
Riesen, R.
Riles, K.
Robertson, N. A.
Robinet, F.
Rocchi, A.
Roddy, S.
Rodriguez, C.
Rodruck, M.
Roever, C.
Rolland, L.
Rollins, J. G.
Romano, R.
Romanov, G.
Romie, J. H.
Rosinska, D.
Rowan, S.
Ruedger, A.
Ruggi, P.
Ryan, K.
Salemi, F.
Sammut, L.
Sandberg, V.
Sanders, J.
Sannibale, V.
Santiago-Prieto, I.
Saracco, E.
Sassolas, B.
Sathyaprakash, B. S.
Saulson, P. R.
Savage, R.
Schilling, R.
Schnabel, R.
Schofield, R. M. S.
Schreiber, E.
Schuette, D.
Schulz, B.
Schutz, B. F.
Schwinberg, P.
Scott, J.
Scott, S. M.
Seifert, F.
Sellers, D.
Sengupta, A. S.
Sentenac, D.
Sergeev, A.
Shaddock, D.
Shah, S.
Shahriar, M. S.
Shaltev, M.
Shapiro, B.
Shawhan, P.
Shoemaker, D. H.
Sidery, T. L.
Siellez, K.
Siemens, X.
Sigg, D.
Simakov, D.
Singer, A.
Singer, L.
Sintes, A. M.
Skelton, G. R.
Slagmolen, B. J. J.
Slutsky, J.
Smith, J. R.
Smith, M. R.
Smith, R. J. E.
Smith-Lefebvre, N. D.
Soden, K.
Son, E. J.
Sorazu, B.
Souradeep, T.
Sperandio, L.
Staley, A.
Steinert, E.
Steinlechner, J.
Steinlechner, S.
Steplewski, S.
Stevens, D.
Stochino, A.
Stone, R.
Strain, K. A.
Straniero, N.
Strigin, S.
Stroeer, A. S.
Sturani, R.
Stuver, A. L.
Summerscales, T. Z.
Susmithan, S.
Sutton, P. J.
Swinkels, B.
Szeifert, G.
Tacca, M.
Talukder, D.
Tang, L.
Tanner, D. B.
Tarabrin, S. P.
Taylor, R.
ter Braack, A. P. M.
Thirugnanasambandam, M. P.
Thomas, M.
Thomas, P.
Thorne, K. A.
Thorne, K. S.
Thrane, E.
Tiwari, V.
Tokmakov, K. V.
Tomlinson, C.
Toncelli, A.
Tonelli, M.
Torre, O.
Torres, C. V.
Torrie, C. I.
Travasso, F.
Traylor, G.
Tse, M.
Ugolini, D.
Unnikrishnan, C. S.
Vahlbruch, H.
Vajente, G.
Vallisneri, M.
Van den Brand, J. F. J.
Van Den Broeck, C.
van der Putten, S.
van der Sluys, M. V.
van Heijningen, J.
van Veggel, A. A.
Vass, S.
Vasuth, M.
Vaulin, R.
Vecchio, A.
Vedovato, G.
Veitch, J.
Veitch, P. J.
Venkateswara, K.
Verma, S.
Vetrano, F.
Vicere, A.
Vincent-Finley, R.
Vinet, J. -Y.
Vitale, S.
Vlcek, B.
Vo, T.
Vocca, H.
Vorvick, C.
Vousden, W. D.
Vrinceanu, D.
Vyachanin, S. P.
Wade, A.
Wade, L.
Wade, M.
Waldman, S. J.
Walker, M.
Wallace, L.
Wan, Y.
Wang, J.
Wang, M.
Wang, X.
Wanner, A.
Ward, R. L.
Was, M.
Weaver, B.
Wei, L. -W.
Weinert, M.
Weinstein, A. J.
Weiss, R.
Welborn, T.
Wen, L.
Wessels, P.
West, M.
Westphal, T.
Wette, K.
Whelan, J. T.
Whitcomb, S. E.
White, D. J.
Whiting, B. F.
Wibowo, S.
Wiesner, K.
Wilkinson, C.
Williams, L.
Williams, R.
Williams, T.
Willis, J. L.
Willke, B.
Wimmer, M.
Winkelmann, L.
Winkler, W.
Wipf, C. C.
Wittel, H.
Woan, G.
Worden, J.
Yablon, J.
Yakushin, I.
Yamamoto, H.
Yancey, C. C.
Yang, H.
Yeaton-Massey, D.
Yoshida, S.
Yum, H.
Yvert, M.
Zadrozny, A.
Zanolin, M.
Zendri, J. -P.
Zhang, F.
Zhang, L.
Zhao, C.
Zhu, H.
Zhu, X. J.
Zotov, N.
Zucker, M. E.
Zweizig, J.
CA LIGO Sci Collaboration
Virgo Collaboration
TI Constraints on Cosmic Strings from the LIGO-Virgo Gravitational-Wave
Detectors
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID INFLATION; LIMITS
AB Cosmic strings can give rise to a large variety of interesting astrophysical phenomena. Among them, powerful bursts of gravitational waves (GWs) produced by cusps are a promising observational signature. In this Letter we present a search for GWs from cosmic string cusps in data collected by the LIGO and Virgo gravitational wave detectors between 2005 and 2010, with over 625 days of live time. We find no evidence of GW signals from cosmic strings. From this result, we derive new constraints on cosmic string parameters, which complement and improve existing limits from previous searches for a stochastic background of GWs from cosmic microwave background measurements and pulsar timing data. In particular, if the size of loops is given by the gravitational backreaction scale, we place upper limits on the string tension G mu below 10-8 in some regions of the cosmic string parameter space.
C1 [Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Ajith, P.; Anderson, R. A.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Barayoga, J. C.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chakraborty, R.; Chalermsongsak, T.; Coyne, D. C.; Daudert, B.; Dergachev, V.; Driggers, J. C.; Ehrens, P.; Etzel, T.; Fotopoulos, N.; Gushwa, K. E.; Gustafson, E. K.; Hall, E.; Harms, J.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D.; Lazzarini, A.; Lewis, J. B.; Litvine, V.; Lloyd, D.; Mageswaran, M.; Mailand, K.; Maros, E.; Martynov, D.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Nash, T.; Ogin, G. H.; Osthelder, C.; Pedraza, M.; Phelps, M.; Poux, C.; Price, L. R.; Privitera, S.; Quintero, E.; Raymond, V.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Seifert, F.; Singer, A.; Singer, L.; Smith, M. R.; Smith-Lefebvre, N. D.; Taylor, R.; Thirugnanasambandam, M. P.; Thrane, E.; Torrie, C. I.; Vass, S.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Williams, R.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Abbott, T.; Bowers, J.; Corbitt, T. R.; DeRosa, R.; Effler, A.; Giaime, J. A.; Gonzalez, G.; Iafrate, J.; Johnson, W. W.; Kokeyama, K.; Kudla, S.; May, G.; Mullavey, A.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Accadia, T.; Bebronne, M.; Buskulic, D.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Yvert, M.] Univ Savoie, CNRS IN2P3, LAPP, F-74941 Annecy Le Vieux, France.
[Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Garufi, F.; Milano, L.; Romano, R.] Complesso Univ Monte S Angelo, Ist Nazl Fis Nucl, Sez Napoli, 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.; Doravari, S.; Evans, T.; Feldbaum, D.; Forsi, E.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Guido, C.; Hanson, J.; Heintze, M.; 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.; Thomas, M.; Thorne, K. A.; Traylor, G.; Welborn, T.; Yakushin, I.] Livingston Observ, LIGO, Livingston, LA 70754 USA.
[Adams, T.; Edwards, M.; Fairhurst, S.; Macdonald, E.; Macleod, D. M.; Nuttall, L. K.; Ohme, F.; Predoi, V.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Affeldt, C.; Allen, B.; Aulbert, C.; Bauchrowitz, J.; Bergmann, G.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Dahl, K.; Dal Canton, T.; Damjanic, M.; Danzmann, K.; Denker, T.; Dent, T.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Hanke, M.; Heurs, M.; Kawazoe, F.; Keitel, D.; Keppel, D. G.; Khalaidovski, A.; Koehlenbeck, S.; Kringel, V.; Kuehn, G.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Manca, G. M.; Mazzolo, G.; Mehmet, M.; Mokler, F.; Mossavi, K.; Mow-Lowry, C. M.; Oppermann, P.; Pickenpack, M.; Poeld, J.; Prijatelj, M.; Prix, R.; Roever, C.; Ruedger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schreiber, E.; Schuette, D.; Schulz, B.; Shaltev, M.; Simakov, D.; Slutsky, J.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Wanner, A.; Was, M.; 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.
[Agathos, M.; Bauer, Th. S.; Beker, M. G.; Bertolini, A.; Blom, M.; Bulten, H. J.; Del Pozzo, W.; Jonker, R. J. G.; Li, T. G. F.; Meidam, J.; Nelemans, G.; Rabeling, D. S.; Shah, S.; ter Braack, A. P. M.; Van den Brand, J. F. J.; Van Den Broeck, C.; van der Putten, S.; van der Sluys, M. V.; van Heijningen, J.; Veitch, J.; Vitale, S.] Nikhef, NL-1098 XG Amsterdam, Netherlands.
[Aggarwal, N.; Barnum, S. H.; Barsotti, L.; Bodiya, T. P.; Donovan, F.; Essick, R.; Evans, M.; Foley, S.; Fritschel, P.; Gras, S.; Isogai, T.; Katsavounidis, E.; Kissel, J. S.; Kwee, P.; Lee, J.; MacInnis, M.; Mason, K.; Matichard, F.; Mavalvala, N.; Mittleman, R.; Oelker, E.; Shoemaker, D. H.; Vaulin, R.; Vitale, S.; Waldman, S. J.; Weiss, R.; Wipf, C. C.; Zhang, F.; Zucker, M. E.] MIT, LIGO, Cambridge, MA 02139 USA.
[Aguiar, O. D.; Constancio, M., Jr.; Costa, C. A.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Allen, B.; Ceron, E. Amador; Anderson, W. G.; Brady, P. R.; Caudill, S.; Creighton, J. D. E.; Giampanis, S.; Hammer, D.; Huynh, M.; Kline, J.; Koranda, S.; Mercer, R. A.; Moe, B.; Ochsner, E.; O'Shaughnessy, R.; Pankow, C.; Papa, M. A.; Siemens, X.; Skelton, G. R.; Soden, K.; Vlcek, B.; Wade, L.; Wade, M.; Wibowo, S.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Allen, B.; Ast, S.; Aufmuth, P.; Danzmann, K.; Kaufer, H.; Lueck, H.; Meier, T.; Schnabel, R.; Vahlbruch, H.; Willke, B.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Allocca, A.; Basti, A.; Bitossi, M.; Bonelli, L.; Boschi, V.; Bradaschia, C.; Cella, G.; 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.
[Allocca, A.; Paoletti, R.; Torre, O.] Univ Siena, I-53100 Siena, Italy.
[Amariutei, D.; Ciani, G.; Deleeuw, E.; Eichholz, J.; Eikenberry, S. S.; Feldbaum, D.; Fulda, P.; Gleason, J.; Goetz, R.; Hartman, M. T.; Heintze, M.; Klimenko, S.; Liu, Z.; Martin, R. M.; Mitselmakher, G.; Moraru, D.; Moreno, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Kumar, D. Nanda; Necula, V.; Ottens, R. S.; Reitze, D. H.; Tanner, D. B.; Tiwari, V.; Whiting, B. F.; Williams, L.] Univ Florida, Gainesville, FL 32611 USA.
[Arceneaux, C.; Cavaglia, M.; Dietz, A.] Univ Mississippi, University, MS 38677 USA.
[Areeda, J.; Foley, E.; Griffo, C.; Lee, J.; Lockett, V.; Magana-Sandoval, F.; Padilla, C.; Smith, J. R.] Calif State Univ Fullerton, Fullerton, CA 92831 USA.
[Astone, P.; Colla, A.; Conte, A.; Frasca, S.; Majorana, E.; Mangano, V.; Nardecchia, I.; Naticchioni, L.; Palomba, C.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
[Aylott, B. E.; Bond, C.; Brown, D. D.; Brueckner, F.; Carbone, L.; Freise, A.; Grover, K.; Lodhia, D.; Mandel, I.; Mingarelli, C. M. F.; Sidery, T. L.; Smith, R. J. E.; Vecchio, A.; Vousden, W. D.; Wang, M.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Babak, S.; Behnke, B.; Grunewald, S.; Leaci, P.; Papa, M. A.; Schutz, B. F.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Baker, P. T.; Cornish, N.] Montana State Univ, Bozeman, MT 59717 USA.
[Ballardin, G.; Canuel, B.; Carbognani, F.; Cavalieri, R.; Chiummo, A.; Cuoco, E.; Dattilo, V.; Day, R.; Fiori, I.; Genin, E.; Hemming, G.; Kasprzack, M.; Marque, J.; Mohan, M.; Nocera, F.; Paoletti, F.; Pasqualetti, A.; Ruggi, P.; Sentenac, D.; Swinkels, B.; Zendri, J. -P.] EGO, I-56021 Pisa, Italy.
[Ballmer, S. W.; Brown, D. A.; Couvares, P.; Fisher, R.; Harry, I. W.; Huerta, E. A.; Kelley, D. B.; Kumar, P.; Lough, J.; Massinger, T. J.; Mohapatra, S. R. P.; Nitz, A.; Perreca, A.; Saulson, P. R.; West, M.] Syracuse Univ, Syracuse, NY 13244 USA.
[Barker, D.; Barton, M. A.; Batch, J.; Berliner, J. M.; Clara, F.; Cook, D.; Dwyer, S.; Garcia, J.; Gray, C.; Hanks, J.; Hoak, D.; Ingram, D. R.; Izumi, K.; Jones, D.; Kawabe, K.; Landry, M.; Levine, B.; Lhuillier, V.; Lubinski, M. J.; McCarthy, R.; Mendell, G.; Paris, H.; Raab, F. J.; Radkins, H.; Reed, C. M.; Rodruck, M.; Ryan, K.; Sandberg, V.; Savage, R.; Schwinberg, P.; Sigg, D.; Steinert, E.; Thomas, P.; Vo, T.; Vorvick, C.; Weaver, B.; Wilkinson, C.; Worden, J.] Hanford Observ, LIGO, Richland, WA 99352 USA.
[Barr, B.; Bassiri, R.; Bell, A. S.; Bell, C.; Campsie, P.; Craig, K.; Cumming, A.; Cunningham, L.; Davies, G. S.; Evans, K.; Gill, C.; Gordon, N.; Grant, A.; Hammond, G.; Haughian, K.; Hendry, M.; Heng, I. S.; Hild, S.; Hough, J.; Hu, Y.; Huttner, S. H.; Jones, R.; Kumar, R.; Lawrie, C.; Logue, J.; Macarthur, J.; Martin, I. W.; Messenger, C.; Murray, P. G.; Newton, G.; Pitkin, M.; Robertson, N. A.; Rowan, S.; Santiago-Prieto, I.; Scott, J.; Sorazu, B.; Strain, K. A.; Torrie, C. I.; van Veggel, A. A.; Woan, G.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Barsuglia, M.; Buy, C.; Chassande-Mottin, E.; Tacca, M.] Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, APC,CNRS,IN2P3,CEA Irfu, F-75205 Paris 13, France.
[Bartos, I.; Belopolski, I.; Countryman, S.; Factourovich, M.; Marka, S.; Marka, Z.; Matone, L.; Murphy, D.; Raffai, P.; Staley, A.; Tse, M.] Columbia Univ, New York, NY 10027 USA.
[Bassiri, R.; Bhadbhade, T.; Byer, R. L.; Clark, D. E.; Kim, N.; Kucharczyk, C.; Kurdyumov, R.; Lantz, B.; Lin, A. C.; Markosyan, A.; Shapiro, B.] Stanford Univ, Stanford, CA 94305 USA.
[Basti, A.; Bonelli, L.; Di Lieto, A.; Ferrini, F.; Fidecaro, F.; Passaquieti, R.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Vajente, G.] Univ Pisa, I-56127 Pisa, Italy.
[Bejger, M.; Rosinska, D.] CAMK PAN, PL-00716 Warsaw, Poland.
[Bersanetti, D.; Chincarini, A.; Farinon, S.; Gemme, G.; Neri, M.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy.
[Bersanetti, D.; Neri, M.] Univ Genoa, I-16146 Genoa, Italy.
[Bessis, D.; Creighton, T. D.; Daveloza, H.; Diaz, M.; Morgado, N.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E.; Larcher, W. Ortega; Puncken, O.; Quetschke, V.; Rakhmanov, M.; Stone, R.; Stroeer, A. S.; Tang, L.; Torres, C. V.; Vrinceanu, D.] 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.; Dmitry, K.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L.; Strigin, S.; Vyachanin, 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.] Univ Paris 11, NASA, IN2P3, CNRS, F-91898 Orsay, France.
[Blackburn, L.; Camp, J. B.; Gehrels, N.; Graff, P. B.; Kanner, J. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blair, D.; Chen, X.; Chu, Q.; Chung, S.; Coward, D. M.; Danilishin, S. L.; Dumas, J. -C.; Fang, Q.; Hooper, S.; Howell, E. J.; Ju, L.; Susmithan, S.; Verma, S.; Wen, L.; Whitcomb, S. E.; Zhao, C.; Zhu, X. J.] Univ Western Australia, Crawley, WA 6009, Australia.
[Boer, M.; Brillet, A.; Coulon, J. -P.; Dereli, H.; Fournier, J. -D.; Heitmann, H.; Kefelian, F.; Man, N.; Martinelli, L.; Meacher, D.; Pichot, M.; Regimbau, T.; Siellez, K.; Vinet, J. -Y.; Wei, L. -W.] Univ Rennes 1, Univ Nice Sophia Antipolis, CNRS, F-06304 Nice, France.
[Bondu, F.] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France.
[Bonnand, R.; Cagnoli, G.; Degallaix, J.; Flaminio, R.; Granata, M.; Michel, C.; Pinard, L.; Saracco, E.; Sassolas, B.; Straniero, N.] Univ Lyon, IN2P3 CNRS, LMA, F-69622 Villeurbanne, France.
[Bose, S.; Brannen, C. A.; Dayanga, T.; Ghosh, S.; Hall, B.; Poole, V.; Steplewski, S.] Washington State Univ, Washington, DC 99164 USA.
[Bosi, L.; Colombini, M.; Gammaitoni, L.; Marchesoni, F.; Neri, I.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Branchesi, M.; Guidi, G. M.; Losurdo, G.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Florence, Italy.
[Branchesi, M.; Guidi, G. M.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Univ Urbino Carlo Bo, I-61029 Urbino, Italy.
[Brau, J. E.; Frey, R.; Harstad, E. D.; Quitzow-James, R.; Schofield, R. M. S.; Talukder, D.] Univ Oregon, Eugene, OR 97403 USA.
[Briant, T.; Cohadon, P. -F.; Deleglise, S.; Heidmann, A.] Univ Paris 06, CNRS, ENS, Lab Kastler Brossel, F-75005 Paris, France.
[Bulik, T.; Kowalska, I.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
[Bulten, H. J.; Cleva, F.; Rabeling, D. S.; Van den Brand, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands.
[Buonanno, A.; Capano, C. D.; Pan, Y.; Shawhan, P.; Yancey, C. C.] Univ Maryland, College Pk, MD 20742 USA.
[Cadonati, L.; Clark, J. A.; Lombardi, A. L.; McIver, J.] Univ Massachusetts, Amherst, MA 01003 USA.
[Calderon Bustillo, J.; Gil-Casanova, S.; Husa, S.; Jimenez-Forteza, F.; Sintes, A. M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain.
[Calloni, E.; De Rosa, R.; Garufi, F.; Milano, L.] Univ Naples Federico II, Complesso Univ Monte S Angelo, I-80126 Naples, Italy.
[Cannon, K. C.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Cao, J.; Du, Z.; Hua, Z.; Lebigot, E. O.; Liu, Y.; Wan, Y.; Wang, X.] Tsinghua Univ, Beijing 100084, Peoples R China.
[Caride, S.; Gustafson, R.; Meadors, G. D.; Riles, K.; Sanders, J.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Castiglia, A.; Frei, M.; Mohapatra, S. R. P.; Peiris, P.; Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Cesarini, E.; D'Antonio, S.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Minenkov, Y.; Re, V.; Rocchi, A.; Sperandio, L.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Chao, S.; Huang, V.; Ou, J.; Wang, J.] Natl Tsing Hua Univ, Hsinchu 300, Taiwan.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Chen, Y.; Gossan, S.; Hong, T.; Kaufman, K.; Luan, J.; Miao, H.; Ott, C. D.; Thorne, K. S.; Vallisneri, M.; Yang, H.] CALTECH, CaRT, Pasadena, CA 91125 USA.
[Cho, H. S.; Kim, Y. -M.; Lee, C. -H.] Pusan Natl Univ, Pusan 609735, South Korea.
[Chow, J.; Chua, S. S. Y.; Inta, R.; McClelland, D. E.; Miller, J.; Nguyen, T.; Scott, S. M.; Shaddock, D.; Slagmolen, B. J. J.; Stochino, A.; Wade, A.; Ward, R. L.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Christensen, N.] Carleton Coll, Northfield, MN 55057 USA.
[Coccia, E.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy.
[Coccia, E.; Fafone, V.; Re, V.; Sperandio, L.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Colla, A.; Conte, A.; Frasca, S.; Mangano, V.; Naticchioni, L.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Conte, R.; DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[Conte, R.; DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Corsi, A.] George Washington Univ, Washington, DC 20052 USA.
[Coughlin, M. W.; Gair, J.] Univ Cambridge, Cambridge CB2 1TN, England.
[Crowder, S. G.; Kandhasamy, S.; Kremin, A.; Mandic, V.; Prestegard, T.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Daw, E. J.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[Debreczeni, G.; Endroczi, G.; Nagy, M. F.; Racz, I.; Vasuth, M.] RMKI, Wigner RCP, H-1121 Budapest, Hungary.
[Dhurandhar, S.; Mitra, S.; Souradeep, T.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Drago, M.; Leonardi, M.; Prodi, G. A.] Ist Nazl Fis Nucl, Grp Coll Trento, I-38050 Povo, Trento, Italy.
[Drago, M.; Leonardi, M.; Prodi, G. A.] Univ Trento, I-38050 Povo, Trento, Italy.
[Drever, R. W. P.] CALTECH, Pasadena, CA 91125 USA.
[Farr, B.; Farr, W.; Fazi, D.; Jang, Y. J.; Kalogera, V.; Littenberg, T. B.; Rodriguez, C.; Shahriar, M. S.; Stevens, D.; Yablon, J.; Yum, H.] Northwestern Univ, Evanston, IL 60208 USA.
[Favata, M.] Montclair State Univ, Montclair, NJ 07043 USA.
[Finn, L. S.; Owen, B. J.; Zhu, H.] Penn State Univ, University Pk, PA 16802 USA.
[Frei, Z.; Gergely, L.; Gondan, L.; Raffai, P.; Szeifert, G.] Eotvos Lorand Univ, MTA, H-1117 Budapest, Hungary.
[Fujimoto, M. -K.; Hayama, K.; Kawamura, S.; Mori, T.; Nishida, E.; Nishizawa, A.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Gammaitoni, L.; Neri, I.; Travasso, F.; Vocca, H.] Univ Perugia, I-06123 Perugia, Italy.
[Greenhalgh, R. J. S.; O'Dell, J.] HSIC, Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Gretarsson, A. M.; Hughey, B.; Loew, K.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Groot, P.; Nelemans, G.; Shah, S.; van der Sluys, M. V.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
[Hanna, C.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Harry, G. M.] Amer Univ, Washington, DC 20016 USA.
[Holtrop, M.] Univ New Hampshire, Durham, NH 03824 USA.
[Horrom, T.; Mikhailov, E. E.; Romanov, G.] Coll William & Mary, Williamsburg, VA 23187 USA.
[Hosken, D. J.; Kim, W.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Iyer, B. R.] Raman Res Inst, Bangalore 560080, Karnataka, India.
[Jang, H.; Kang, G.; Kim, B. K.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea.
[Jaranowski, P.] Bialystok Univ, PL-15424 Bialystok, Poland.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Haris, K.; Mazumder, N.; Pai, A.] IISER TVM, Trivandrum 695016, Kerala, India.
[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.; Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Krolak, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Kumar, A.] Inst Plasma Res, Bhat 382428, Gandhinagar, India.
[Larson, S.] Utah State Univ, Logan, UT 84322 USA.
[Lasky, P. D.; Melatos, A.; Pindor, B.; Sammut, L.] Univ Melbourne, Melbourne, Vic 3010, Australia.
[Liu, F.; Liu, H.] Univ Brussels, B-1050 Brussels, Belgium.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy.
[Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA.
[McGuire, S. C.; Vincent-Finley, R.] Southern Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.; Vincent-Finley, R.] A&M Coll, Baton Rouge, LA 70813 USA.
[Nayak, R.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Taejon 305390, South Korea.
[Raja, S.] RRCAT, Indore 452013, Madhya Pradesh, India.
[Rajalakshmi, G.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
[Reid, S.] Univ W Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland.
[Rosinska, D.] Astron Inst, PL-65265 Zielona Gora, Poland.
[Sengupta, A. S.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Vedovato, G.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Williams, T.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
[Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI Losurdo, Giovanni/K-1241-2014; Steinlechner, Sebastian/D-5781-2013;
Kumar, Prem/B-6691-2009; Hild, Stefan/A-3864-2010; Danilishin,
Stefan/K-7262-2012; Gammaitoni, Luca/B-5375-2009; Iyer, Bala
R./E-2894-2012; 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; Ward, Robert/I-8032-2014; Bilenko, Igor/D-5172-2012;
Costa, Cesar/G-7588-2012; Huerta, Eliu/J-5426-2014; CONTE,
ANDREA/J-6667-2012; Salemi, Francesco/F-6988-2014; prodi,
giovanni/B-4398-2010; Prokhorov, Leonid/I-2953-2012; Gorodetsky,
Michael/C-5938-2008; Strigin, Sergey/I-8337-2012; Mitrofanov,
Valery/D-8501-2012; Gemme, Gianluca/C-7233-2008; Bell,
Angus/E-7312-2011; Nelemans, Gijs/D-3177-2012; Leonardi,
Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012;
Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Ottaway,
David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise,
Samuel/B-1599-2015; Neri, Igor/F-1482-2010; Aggarwal, Nancy/M-7203-2015;
Shaddock, Daniel/A-7534-2011; Vicere, Andrea/J-1742-2012; Rocchi,
Alessio/O-9499-2015; Pinto, Innocenzo/L-3520-2016; Ferrante,
Isidoro/F-1017-2012; Bondu, Francois/A-2071-2012; 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; 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; Harms,
Jan/J-4359-2012; Martelli, Filippo/P-4041-2015; Branchesi,
Marica/P-2296-2015; Strain, Kenneth/D-5236-2011; Miao,
Haixing/O-1300-2013; Howell, Eric/H-5072-2014; Gehring,
Tobias/A-8596-2016; Heidmann, Antoine/G-4295-2016; Ott,
Christian/G-2651-2011; Marchesoni, Fabio/A-1920-2008; Zhu,
Xingjiang/E-1501-2016; Frasconi, Franco/K-1068-2016; Groot,
Paul/K-4391-2016
OI 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; Allen,
Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Vitale,
Salvatore/0000-0003-2700-0767; Kanner, Jonah/0000-0001-8115-0577;
Freise, Andreas/0000-0001-6586-9901; Nitz,
Alexander/0000-0002-1850-4587; Sorazu, Borja/0000-0002-6178-3198;
Zweizig, John/0000-0002-1521-3397; Del Pozzo,
Walter/0000-0003-3978-2030; O'Shaughnessy, Richard/0000-0001-5832-8517;
Pierro, Vincenzo/0000-0002-6020-5521; Coccia,
Eugenio/0000-0002-6669-5787; Vetrano, Flavio/0000-0002-7523-4296;
Denker, Timo/0000-0003-1259-5315; Naticchioni, Luca/0000-0003-2918-0730;
calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515;
Boschi, Valerio/0000-0001-8665-2293; Matichard,
Fabrice/0000-0001-8982-8418; Husa, Sascha/0000-0002-0445-1971; Papa,
M.Alessandra/0000-0002-1007-5298; Vocca, Helios/0000-0002-1200-3917;
Aulbert, Carsten/0000-0002-1481-8319; Pinto, Innocenzo
M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Guidi,
Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431; Losurdo,
Giovanni/0000-0003-0452-746X; Steinlechner,
Sebastian/0000-0003-4710-8548; Danilishin, Stefan/0000-0001-7758-7493;
Gammaitoni, Luca/0000-0002-4972-7062; Iyer, Bala R./0000-0002-4141-5179;
Lee, Chang-Hwan/0000-0003-3221-1171; McClelland,
David/0000-0001-6210-5842; Vecchio, Alberto/0000-0002-6254-1617;
Vedovato, Gabriele/0000-0001-7226-1320; Swinkels,
Bas/0000-0002-3066-3601; Ward, Robert/0000-0001-5503-5241; Ricci,
Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576; Fairhurst,
Stephen/0000-0001-8480-1961; prodi, giovanni/0000-0001-5256-915X;
Gorodetsky, Michael/0000-0002-5159-2742; Gemme,
Gianluca/0000-0002-1127-7406; Bell, Angus/0000-0003-1523-0821; Nelemans,
Gijs/0000-0002-0752-2974; Sigg, Daniel/0000-0003-4606-6526; Puppo,
Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef,
Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168;
Deleglise, Samuel/0000-0002-8680-5170; Neri, Igor/0000-0002-9047-9822;
Shaddock, Daniel/0000-0002-6885-3494; Vicere,
Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016;
Ferrante, Isidoro/0000-0002-0083-7228; Bondu,
Francois/0000-0001-6487-5197; 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; Martelli, Filippo/0000-0003-3761-8616;
Strain, Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958;
Howell, Eric/0000-0001-7891-2817; Gehring, Tobias/0000-0002-4311-2593;
Heidmann, Antoine/0000-0002-0784-5175; Ott,
Christian/0000-0003-4993-2055; Marchesoni, Fabio/0000-0001-9240-6793;
Zhu, Xingjiang/0000-0001-7049-6468; Frasconi,
Franco/0000-0003-4204-6587; Groot, Paul/0000-0002-4488-726X
FU United States National Science Foundation; Science and Technology
Facilities Council of the United Kingdom; Max-Planck-Society; State of
Niedersachsen/Germany; 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;
the 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; OTKA of
Hungary; Lyon Institute of Origins (LIO); 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, OTKA of Hungary, the Lyon
Institute of Origins (LIO), the National Research Foundation of Korea,
Industry Canada and the Province of Ontario through the Ministry of
Economic Development and Innovation, the 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 43
TC 25
Z9 25
U1 6
U2 64
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 4
PY 2014
VL 112
IS 13
AR 131101
DI 10.1103/PhysRevLett.112.131101
PG 10
WC Physics, Multidisciplinary
SC Physics
GA AE9PJ
UT WOS:000334339800002
PM 24745400
ER
PT J
AU Iess, L
Stevenson, DJ
Parisi, M
Hemingway, D
Jacobson, RA
Lunine, JI
Nimmo, F
Armstrong, JW
Asmar, SW
Ducci, M
Tortora, P
AF Iess, L.
Stevenson, D. J.
Parisi, M.
Hemingway, D.
Jacobson, R. A.
Lunine, J. I.
Nimmo, F.
Armstrong, J. W.
Asmar, S. W.
Ducci, M.
Tortora, P.
TI The Gravity Field and Interior Structure of Enceladus
SO SCIENCE
LA English
DT Article
ID WATER RESERVOIR; SOUTH-POLE; TITAN; PLUME
AB The small and active Saturnian moon Enceladus is one of the primary targets of the Cassini mission. We determined the quadrupole gravity field of Enceladus and its hemispherical asymmetry using Doppler data from three spacecraft flybys. Our results indicate the presence of a negative mass anomaly in the south-polar region, largely compensated by a positive subsurface anomaly compatible with the presence of a regional subsurface sea at depths of 30 to 40 kilometers and extending up to south latitudes of about 50 degrees. The estimated values for the largest quadrupole harmonic coefficients (10(6)J(2) = 5435.2 +/- 34.9, 10(6)C(22) = 1549.8 +/- 15.6, 1 sigma) and their ratio (J(2)/C-22 = 3.51 +/- 0.05) indicate that the body deviates mildly from hydrostatic equilibrium. The moment of inertia is around 0.335MR(2), where M is the mass and R is the radius, suggesting a differentiated body with a low-density core.
C1 [Iess, L.; Parisi, M.; Ducci, M.] Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerospaziale, I-00184 Rome, Italy.
[Stevenson, D. J.] CALTECH, Pasadena, CA 91125 USA.
[Hemingway, D.; Nimmo, F.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Jacobson, R. A.; Armstrong, J. W.; Asmar, S. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lunine, J. I.] Cornell Univ, Dept Astron, Ithaca, NY 14850 USA.
[Tortora, P.] Univ Bologna, Dipartimento Ingn Ind, I-47121 Forli, Italy.
RP Iess, L (reprint author), Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerospaziale, Via Eudossiana 18, I-00184 Rome, Italy.
EM luciano.iess@uniroma1.it
RI Hemingway, Douglas/F-6332-2014; IESS, Luciano/F-4902-2011
OI Hemingway, Douglas/0000-0001-5617-207X; IESS,
Luciano/0000-0002-6230-5825
FU Italian Space Agency; NASA
FX L.I., M.P., M.D., and P.T. acknowledge support from the Italian Space
Agency. D.H., F.N., and J.I.L. are grateful to NASA for support through
the Cassini Project. The work of R.A.J., J.W.A., and S.W.A. was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. The Doppler data and ancillary
information used in this analysis are archived in NASA's Planetary Data
System.
NR 21
TC 48
Z9 49
U1 10
U2 67
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD APR 4
PY 2014
VL 344
IS 6179
BP 78
EP 80
DI 10.1126/science.1250551
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AE1RD
UT WOS:000333746100055
PM 24700854
ER
PT J
AU Muller, CL
Kidd, C
AF Muller, Catherine L.
Kidd, Chris
TI Debugging geographers: teaching programming to non-computer scientists
SO JOURNAL OF GEOGRAPHY IN HIGHER EDUCATION
LA English
DT Article
DE FORTRAN programming; R; Linux; module design; meteorology; postgraduate
teaching in geography
ID STUDENTS
AB The steep learning curve associated with computer programming can be a daunting prospect, particularly for those not well aligned with this way of logical thinking. However, programming is a skill that is becoming increasingly important. Geography graduates entering careers in atmospheric science are one example of a particularly diverse group who often require a better knowledge and understanding of computing. Critically, there is a necessity in the field for people with a diverse range of data analysis and modelling abilities. This article outlines the module design and evaluation of an introductory programming course for non-computer scientists within a UK geography department.
C1 [Muller, Catherine L.] Univ Birmingham Edgbaston, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England.
[Kidd, Chris] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Kidd, Chris] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Muller, CL (reprint author), Univ Birmingham Edgbaston, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England.
EM c.l.muller@bham.ac.uk
RI Muller, Catherine L./E-9744-2011
OI Muller, Catherine L./0000-0002-5176-5949
NR 44
TC 5
Z9 5
U1 0
U2 7
PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND
SN 0309-8265
EI 1466-1845
J9 J GEOGR HIGHER EDUC
JI J. Geogr. High. Educ.
PD APR 3
PY 2014
VL 38
IS 2
BP 175
EP 192
DI 10.1080/03098265.2014.908275
PG 18
WC Education & Educational Research; Geography
SC Education & Educational Research; Geography
GA AG1TH
UT WOS:000335198500002
ER
PT J
AU Potter, C
AF Potter, Christopher
TI Global assessment of damage to coastal ecosystem vegetation from
tropical storms
SO REMOTE SENSING LETTERS
LA English
DT Article
ID HURRICANE-FIRE INTERACTIONS; RECENT HISTORY; FOREST; DISTURBANCES;
HYPOTHESIS; YUCATAN; MEXICO; IMPACT; RECORD
AB This study reports on the first comprehensive global assessment of tropical storm (TS) impacts on coastal ecosystem vegetation along the landfall pathways of major hurricanes, cyclones and typhoons using satellite data of land cover vegetation for the years 2006 to 2012. Wind damage has been shown to reduce live vegetation pools of carbon, accelerate ecosystem respiration fluxes of carbon dioxide and thereby represent a potentially significant positive feedback to terrestrial greenhouse gas emissions. Based on quarterly detection of changes in Moderate Resolution Imaging Spectroradiometer (MODIS) satellite vegetation greenness, all major TS pathways during the time period were ranked in terms of area of vegetation damage observed. Comparison of vegetation disturbance area along major TS pathways to average rates of disturbance within the same coastal zones (for years during which no TS activity was observed) verified the satellite capability to detect TS ecosystem impacts.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Potter, C (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM chris.potter@nasa.gov
NR 25
TC 0
Z9 0
U1 2
U2 11
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 2150-704X
EI 2150-7058
J9 REMOTE SENS LETT
JI Remote Sens. Lett.
PD APR 3
PY 2014
VL 5
IS 4
BP 315
EP 322
DI 10.1080/2150704X.2014.902546
PG 8
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA AG0EL
UT WOS:000335088000002
ER
PT J
AU Frost, DA
McAuley, WC
Kluver, B
Wastel, M
Maynard, D
Flagg, TA
AF Frost, Deborah A.
McAuley, W. Carlin
Kluver, Bryon
Wastel, Mike
Maynard, Desmond
Flagg, Thomas A.
TI Methods and Accuracy of Sexing Sockeye Salmon Using Ultrasound for
Captive Broodstock Management
SO NORTH AMERICAN JOURNAL OF AQUACULTURE
LA English
DT Article
ID MATURATIONAL STATUS; PACIFIC SALMON; ULTRASONOGRAPHY; STOCKS
AB Ultrasound has been widely used to noninvasively examine the internal anatomy and reproductive status of many fish species. Since 2003, ultrasonography has been an integral part of broodstock management for Endangered Species Act-listed endangered Redfish Lake Sockeye Salmon Oncorhynchus nerka. Initial ultrasound screenings for each year's broodstock were conducted 3 to 4 months prior to anticipated maturation, before external signs of maturation developed. In keeping with the natural life history of these fish, this permitted the separation of nonmaturing fish from maturing fish so the immature fish could maintain feeding and growth. It also permitted maturing seawater-reared fish to be transferred to freshwater for final maturation. Designing a spawning matrix to maintain genetic diversity requires knowledge of the sex of each fish before spawning. Approximately 1 month prior to spawning, a second ultrasound was performed to verify sex identification and thus ensure the accuracy of the spawning matrix. Over a 9-year period, 2,662 fish were examined. The accuracy of sexing age-3 adult Sockeye Salmon ranged from 94.0% to 100%, with an average of 97.7%, while the accuracy of sexing age-4 adult fish ranged from 92.0% to 100%, with an average of 94.4%. The average accuracy was similar for fish examined in seawater or freshwater (98.1% versus 97.3%, respectively). Ultrasound was shown to be an accurate and effective tool for managing the husbandry of our captive broodstock life history.
Received September 13, 2013; accepted January 2, 2014
C1 [Frost, Deborah A.; McAuley, W. Carlin; Kluver, Bryon; Wastel, Mike; Maynard, Desmond; Flagg, Thomas A.] Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Environm & Fisheries Sci Div, Manchester Res Stn, Manchester, WA 98353 USA.
RP Frost, DA (reprint author), Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Environm & Fisheries Sci Div, Manchester Res Stn, POB 130, Manchester, WA 98353 USA.
EM debbie.frost@noaa.gov
FU BPA
FX This Redfish Lake Sockeye Salmon gene rescue program is a cooperative
between NMFS, the Idaho Department of Fish and Game, the Bonneville
Power Administration (BPA), the Shoshone Bannock Tribes, and others
involved with salmon conservation in the Columbia River Basin. The
program is funded by the BPA and coordinated through the Northwest Power
and Conservation Council's Fish and Wildlife Program. Mention of
specific products does not constitute endorsement by NOAA.
NR 14
TC 1
Z9 2
U1 2
U2 16
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 520 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 1522-2055
EI 1548-8454
J9 N AM J AQUACULT
JI N. Am. J. Aqualcult.
PD APR 3
PY 2014
VL 76
IS 2
BP 153
EP 158
DI 10.1080/15222055.2014.886647
PG 6
WC Fisheries
SC Fisheries
GA AE9NE
UT WOS:000334333700009
ER
PT J
AU Ade, PAR
Akiba, Y
Anthony, AE
Arnold, K
Atlas, M
Barron, D
Boettger, D
Borrill, J
Borys, C
Chapman, S
Chinone, Y
Dobbs, M
Elleflot, T
Errard, J
Fabbian, G
Feng, C
Flanigan, D
Gilbert, A
Grainger, W
Halverson, NW
Hasegawa, M
Hattori, K
Hazumi, M
Holzapfel, WL
Hori, Y
Howard, J
Hyland, P
Inoue, Y
Jaehnig, GC
Jaffe, A
Keating, B
Kermish, Z
Keskitalo, R
Kisner, T
Le Jeune, M
Lee, AT
Leitch, EM
Linder, E
Lungu, M
Matsuda, F
Matsumura, T
Meng, X
Miller, NJ
Morii, H
Moyerman, S
Myers, MJ
Navaroli, M
Nishino, H
Paar, H
Peloton, J
Poletti, D
Quealy, E
Rebeiz, G
Reichardt, CL
Richards, PL
Ross, C
Rotermund, K
Schanning, I
Schenck, DE
Sherwin, BD
Shimizu, A
Shimmin, C
Shimon, M
Siritanasak, P
Smecher, G
Spieler, H
Stebor, N
Steinbach, B
Stompor, R
Suzuki, A
Takakura, S
Tikhomirov, A
Tomaru, T
Wilson, B
Yadav, A
Zahn, O
AF Ade, P. A. R.
Akiba, Y.
Anthony, A. E.
Arnold, K.
Atlas, M.
Barron, D.
Boettger, D.
Borrill, J.
Borys, C.
Chapman, S.
Chinone, Y.
Dobbs, M.
Elleflot, T.
Errard, J.
Fabbian, G.
Feng, C.
Flanigan, D.
Gilbert, A.
Grainger, W.
Halverson, N. W.
Hasegawa, M.
Hattori, K.
Hazumi, M.
Holzapfel, W. L.
Hori, Y.
Howard, J.
Hyland, P.
Inoue, Y.
Jaehnig, G. C.
Jaffe, A.
Keating, B.
Kermish, Z.
Keskitalo, R.
Kisner, T.
Le Jeune, M.
Lee, A. T.
Leitch, E. M.
Linder, E.
Lungu, M.
Matsuda, F.
Matsumura, T.
Meng, X.
Miller, N. J.
Morii, H.
Moyerman, S.
Myers, M. J.
Navaroli, M.
Nishino, H.
Paar, H.
Peloton, J.
Poletti, D.
Quealy, E.
Rebeiz, G.
Reichardt, C. L.
Richards, P. L.
Ross, C.
Rotermund, K.
Schanning, I.
Schenck, D. E.
Sherwin, B. D.
Shimizu, A.
Shimmin, C.
Shimon, M.
Siritanasak, P.
Smecher, G.
Spieler, H.
Stebor, N.
Steinbach, B.
Stompor, R.
Suzuki, A.
Takakura, S.
Tikhomirov, A.
Tomaru, T.
Wilson, B.
Yadav, A.
Zahn, O.
CA POLARBEAR Collaboration
TI Evidence for Gravitational Lensing of the Cosmic Microwave Background
Polarization from Cross-Correlation with the Cosmic Infrared Background
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID SOUTH-POLE TELESCOPE; POWER SPECTRUM; HERSCHEL ATLAS; DAMPING TAIL;
PROBE; MAPS; SKY; GHZ
AB We reconstruct the gravitational lensing convergence signal from cosmic microwave background (CMB) polarization data taken by the POLARBEAR experiment and cross-correlate it with cosmic infrared background maps from the Herschel satellite. From the cross spectra, we obtain evidence for gravitational lensing of the CMB polarization at a statistical significance of 4.0 sigma and indication of the presence of a lensing B-mode signal at a significance of 2.3 sigma. We demonstrate that our results are not biased by instrumental and astrophysical systematic errors by performing null tests, checks with simulated and real data, and analytical calculations. This measurement of polarization lensing, made via the robust cross-correlation channel, not only reinforces POLARBEAR auto-correlation measurements, but also represents one of the early steps towards establishing CMB polarization lensing as a powerful new probe of cosmology and astrophysics.
C1 [Ade, P. A. R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3XQ, S Glam, Wales.
[Akiba, Y.; Hasegawa, M.; Hazumi, M.; Inoue, Y.; Shimizu, A.] Grad Univ Adv Studies, Kanagawa 2400115, Japan.
[Anthony, A. E.; Halverson, N. W.; Jaehnig, G. C.; Schenck, D. E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Arnold, K.; Atlas, M.; Barron, D.; Boettger, D.; Elleflot, T.; Feng, C.; Keating, B.; Matsuda, F.; Moyerman, S.; Navaroli, M.; Paar, H.; Schanning, I.; Shimon, M.; Siritanasak, P.; Stebor, N.; Wilson, B.; Yadav, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Borrill, J.; Errard, J.; Keskitalo, R.; Kisner, T.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, La Jolla, CA 92093 USA.
[Borrill, J.; Errard, J.; Kisner, T.; Linder, E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Borys, C.] CALTECH, Pasadena, CA 91125 USA.
[Chapman, S.; Ross, C.; Rotermund, K.; Tikhomirov, A.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada.
[Chinone, Y.; Hasegawa, M.; Hattori, K.; Hazumi, M.; Hori, Y.; Matsumura, T.; Morii, H.; Takakura, S.; Tomaru, T.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan.
[Chinone, Y.; Flanigan, D.; Holzapfel, W. L.; Howard, J.; Lee, A. T.; Lungu, M.; Meng, X.; Myers, M. J.; Quealy, E.; Reichardt, C. L.; Richards, P. L.; Sherwin, B. D.; Shimmin, C.; Steinbach, B.; Suzuki, A.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Dobbs, M.; Gilbert, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 0G4, Canada.
[Fabbian, G.; Le Jeune, M.; Peloton, J.; Poletti, D.; Stompor, R.] Univ Paris Diderot, AstroParticule & Cosmol, CNRS IN2P3, CEA Irfu,Obs Paris,Sorbonne Paris Cite, Paris, France.
[Fabbian, G.] Int Sch Adv Studies SISSA, I-34014 Trieste, Italy.
[Flanigan, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Grainger, W.] STFC, Rutherford Appleton Lab, Swindon SN2 1SZ, Wilts, England.
[Anthony, A. E.; Halverson, N. W.; Schenck, D. E.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.; Jaehnig, G. C.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Hazumi, M.; Nishino, H.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Univ WPI, Kashiwa, Chiba 2778583, Japan.
[Howard, J.] Univ Oxford, Dept Phys, Oxford OX1 2JD, England.
[Hyland, P.] Austin Coll, Dept Phys, Sherman, TX 75090 USA.
[Jaffe, A.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England.
[Leitch, E. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Leitch, E. M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Kermish, Z.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Lee, A. T.; Linder, E.; Spieler, H.; Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Miller, N. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Quealy, E.] Napa Valley Coll, Dept Phys, Napa, CA 94558 USA.
[Rebeiz, G.] Univ Calif San Diego, Dept Elect & Comp Engn, La Jolla, CA 92093 USA.
[Sherwin, B. D.] Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA.
[Shimon, M.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Smecher, G.] Three Speed Log Inc, Vancouver, BC V6A 2J8, Canada.
[Takakura, S.] Osaka Univ, Toyonaka, Osaka 5600043, Japan.
RP Sherwin, BD (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
EM sherwin@berkeley.edu
RI Holzapfel, William/I-4836-2015;
OI Fabbian, Giulio/0000-0002-3255-4695; Reichardt,
Christian/0000-0003-2226-9169
FU DOE [DE-AC02-05CH11231]; NSF [AST-0618398, AST-1212230]; MEXT KAKENHI
[21111002]; KEK Cryogenics Science Center; Natural Sciences and
Engineering Research Council and Canadian Institute for Advanced
Research; NASA Postdoctoral Program; Miller Fellowship; Simons
Foundation; Joan and Irwin Jacobs; Comision Nacional de Investigacicn
Cientfica y Tecnologica de Chile (CONICYT)
FX We thank Frank Wuerthwein, Igor Sfiligoi, Terrence Martin, and Robert
Konecny for their insight and support, and thank Nolberto Oyarce and
Jos, Cortes for their invaluable contributions. Calculations were
performed at the Department of Energy Open Science Grid [39] at the
University of California, San Diego, accessed via the GlideinWMS [40],
at Central Computing System, owned and operated by the Computing
Research Center at KEK, and at NERSC which is supported by the DOE under
Contract No. DE-AC02-05CH11231. The POLARBEAR project is funded by the
NSF under Grants No. AST0618398 and No. AST-1212230. The KEK authors
were supported by MEXT KAKENHI Grant No. 21111002, and acknowledge
support from KEK Cryogenics Science Center. The McGill authors
acknowledge funding from the Natural Sciences and Engineering Research
Council and Canadian Institute for Advanced Research. N. M., B. D. S.,
and K. A. acknowledge support from the NASA Postdoctoral Program, a
Miller Fellowship, and the Simons Foundation, respectively. M. S.
gratefully acknowledges support from Joan and Irwin Jacobs. The James Ax
Observatory operates in the Parque Astroncmico Atacama in Northern Chile
under the auspices of the Comisicn Nacional de Investigacicn Cient fica
y Tecnolcgica de Chile (CONICYT). Finally, we acknowledge the tremendous
contributions by Huan Tran to the POLARBEAR project.
NR 39
TC 34
Z9 34
U1 2
U2 9
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 2
PY 2014
VL 112
IS 13
AR 131302
DI 10.1103/PhysRevLett.112.131302
PG 6
WC Physics, Multidisciplinary
SC Physics
GA AE9OP
UT WOS:000334337500006
PM 24745402
ER
PT J
AU Kostas, VI
Stenger, MB
Knapp, CF
Shapiro, R
Wang, SQ
Diedrich, A
Evans, JM
AF Kostas, Vladimir I.
Stenger, Michael B.
Knapp, Charles F.
Shapiro, Robert
Wang, Siqi
Diedrich, Andre
Evans, Joyce M.
TI Cardiovascular Models of Simulated Moon and Mars Gravities: Head-Up Tilt
vs. Lower Body Unweighting
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE alter-G; LBPP; orthostatic intolerance
ID POSITIVE-PRESSURE; ORTHOSTATIC INTOLERANCE; RESPONSES; SPACEFLIGHT;
POSTURE; COUNTERMEASURE; WOMEN; REST
AB Introduction: In this study we compare two models [head-up tilt (HUT) vs. body unweighting using lower body positive pressure (LBPP)] to simulate Moon, Mars, and Earth gravities. A literature search did not reveal any comparisons of this type performed previously. We hypothesized that segmental fluid volume shifts (thorax, abdomen, upper and lower leg), cardiac output, and blood pressure (BP), heart rate (HR), and total peripheral resistance to standing would be similar in the LBPP and HUT models. Methods: There were 21 subjects who were studied while supine (simulation of spaceflight) and standing at 100% (Earth), 40% (Mars), and 20% (Moon) bodyweight produced by LBPP in Alter-G and while supine and tilted at 80, 20, and 100 HUT (analogues of Earth, Mars, and Moon gravities, respectively). Results: Compared to supine, fluid shifts from the chest to the abdomen, increases in HR, and decreases in stroke volume were greater at 100% bodyweight than at reduced weights in response to both LBPP and HUT. Differences between the two models were found for systolic BP, diastolic BP, mean arterial BP, stroke volume, total peripheral resistance, and thorax and abdomen impedances, while HR, cardiac output, and upper and lower leg impedances were similar. Conclusions: Bodyweight unloading via both LBPP and HUT resulted in cardiovascular changes similar to those anticipated in actual reduced gravity environments. The LBPP model/Alter-G has the advantage of providing an environment that allows dynamic activity at reduced body-weight; however, the significant increase in blood pressures in the Alter-G may favor the HUT model.
C1 [Kostas, Vladimir I.; Knapp, Charles F.; Shapiro, Robert; Wang, Siqi; Evans, Joyce M.] Univ Kentucky, Lexington, KY 40506 USA.
[Stenger, Michael B.] NASA, Lyndon B Johnson Space Ctr, Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA.
[Diedrich, Andre] Vanderbilt Univ, Nashville, TN 37235 USA.
RP Evans, JM (reprint author), Univ Kentucky, Ctr Biomed Engn, Rm 1,600 Rose St, Lexington, KY 40506 USA.
EM jevans1@uky.edu
FU KY NASA EPSCoR Research Area [NNX07AT58A, NNX07AL55A]
FX We would like to thank L. Christine Ribeiro (NASA JSC), Elizabeth Salmon
(UK), Dan Irwin (UK), and Matt Haaga (UK) for data analysis and Tim Matz
(NASA JSC) for ultrasound data. This study was supported by KY NASA
EPSCoR Research Area I Grant # NNX07AT58A and Grant # NNX07AL55A.
NR 21
TC 3
Z9 3
U1 1
U2 3
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
EI 1943-4448
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD APR
PY 2014
VL 85
IS 4
BP 414
EP 419
DI 10.3357/ASEM.3687.2014
PG 6
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA CB6FF
UT WOS:000349721600003
PM 24754202
ER
PT J
AU De Witt, JK
Schaffner, G
Ploutz-Snyder, LL
AF De Witt, John K.
Schaffner, Grant
Ploutz-Snyder, Lori L.
TI Bungee Force Level, Stiffness, and Variation During Treadmill Locomotion
in Simulated Microgravity
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE exercise; treadmill; bungee force; countermeasures
ID INTERNATIONAL-SPACE-STATION; FOOT FORCES; EXERCISE; BONE
AB Introduction: Crewmembers performing treadmill exercise on the International Space Station must wear a harness with an external gravity replacement force that is created by elastomer bungees. The quantification of the total external force, displacement, stiffness, and force variation is important for understanding the forces applied to the crewmember during typical exercise. Methods: Data were collected during static trials in the laboratory from a single subject and four subjects were tested while walking at 1.34 m.s(-1) and running at 2.24 m.s(-1) and 3.13 m.s(-1) on a treadmill during simulated microgravity in parabolic flight. The external force was provided by bungees and carabiner clips in configurations commonly used by crewmembers. Total external force, displacement, and force variation in the bungee system were measured, from which stiffness was computed. Results: Mean external force ranged from 431 to 804 N (54-131% bodyweight) across subjects and conditions. Mean displacement was 4 to 8 cm depending upon gait speed. Mean stiffness was affected by bungee configuration and ranged from 1.73 to 29.20 N.cm(-1). Force variation for single bungee configurations was 2.61-4.48% of total external force and between 4.30-57.5% total external force for two-bungee configurations. Conclusions: The external force supplied to crewmembers by elastomer bungees provided a range of loading levels with variations that occur throughout the gait cycle. The quantification of bungee-loading characteristics is important to better define the system currently used by crewmembers during exercise.
C1 [De Witt, John K.] Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA.
Univ Space Res Assoc, Houston, TX USA.
Univ Cincinnati, Cincinnati, OH USA.
NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP De Witt, JK (reprint author), Wyle Sci Technol & Engn Grp, 1290 Hercules,Ste 120, Houston, TX 77058 USA.
EM jolm.k.dewitt@nasa.gov
NR 10
TC 3
Z9 3
U1 0
U2 8
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
EI 1943-4448
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD APR
PY 2014
VL 85
IS 4
BP 449
EP 455
DI 10.3357/ASEM.3217.2014
PG 7
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA CB6FF
UT WOS:000349721600009
PM 24754208
ER
PT J
AU Morgan, J
Heer, M
Hargens, A
Macias, B
Hudson, E
Shackelford, L
Zwart, S
Smith, S
AF Morgan, Jennifer
Heer, Martina
Hargens, Allen
Macias, Brandon
Hudson, Edgar
Shackelford, Linda
Zwart, Sara
Smith, Scott
TI Bone metabolism and renal stone risk during bed rest for men and women
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Experimental Biology Meeting
CY APR 26-30, 2014
CL San Diego, CA
SP Cenveo, LI COR, Wiley, Mead Johnson Pediat Nutr Inst, IPRECIO, F1000 Res, Amer Assoc Anatomists, Amer Physiol Soc, Amer Soc Biochem & Mol Biol, Amer Soc Investigat Pathol, Amer Soc Nutr, Amer Soc Pharmacol & Expt Therapeut
C1 [Hudson, Edgar] JES Tech, Houston, TX USA.
[Shackelford, Linda; Smith, Scott] NASA, Houston, TX USA.
[Morgan, Jennifer] NASA, ORAU, Houston, TX USA.
[Hargens, Allen; Macias, Brandon] Univ Calif San Diego, San Diego, CA USA.
[Heer, Martina] Univ Bonn, Bonn, Germany.
[Zwart, Sara] NASA, USRA, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
EI 1530-6860
J9 FASEB J
JI Faseb J.
PD APR
PY 2014
VL 28
IS 1
SU S
MA 257.8
PG 2
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA AX0MP
UT WOS:000346646700331
ER
PT J
AU Philip, S
Martin, RV
Pierce, JR
Jimenez, JL
Zhang, Q
Canagaratna, MR
Spracklen, DV
Nowlan, CR
Lamsal, LN
Cooper, MJ
Krotkov, NA
AF Philip, S.
Martin, R. V.
Pierce, J. R.
Jimenez, J. L.
Zhang, Q.
Canagaratna, M. R.
Spracklen, D. V.
Nowlan, C. R.
Lamsal, L. N.
Cooper, M. J.
Krotkov, N. A.
TI Spatially and seasonally resolved estimate of the ratio of organic mass
to organic carbon
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Organic aerosol; Organic carbon; NO2; AMS; OMI; GEOS-Chem
ID UNITED-STATES; HYDROCARBON-LIKE; INTEX-B; AEROSOL; SPECTROMETER;
PARTICLES; EMISSIONS; VISIBILITY; CHEMISTRY; PITTSBURGH
AB Particulate organic matter is of interest for air quality and climate research, but the relationship between ambient organic mass (OM) and organic carbon (CC) remains ambiguous both in measurements and in modeling. We present a simple method to derive an estimate of the spatially and seasonally resolved global, lower tropospheric, ratio between OM and CC. We assume ambient NO2 concentrations as a surrogate for fresh emission which mostly determines the continental scale OM/OC ratio. For this, we first develop a parameterization for the OM/OC ratio using the primary organic aerosol (POA) fraction of total OM estimated globally from Aerosol Mass Spectrometer (AMS) measurements, and evaluate it with high mass resolution AMS data. Second, we explore the ability of ground-level NO2 concentrations derived from the OMI satellite sensor to serve as a proxy for fresh emissions that have a high POA fraction, and apply NO2 data to derive ambient POA fraction. The combination of these two methods yields an estimate of OM/OC from NO2 measurements. Although this method has inherent deficiencies over biomass burning, free-tropospheric, and marine environments, elsewhere it offers more information than the currently used global-mean OM/OC ratios. The OMI-derived global OM/OC ratio ranges from 1.3 to 2.1 (mu g/mu gC), with distinct spatial variation between urban and rural regions. The seasonal OM/OC ratio has a summer maximum and a winter minimum over regions dominated by combustion emissions. This dataset serves as a tool for interpreting organic carbon measurements, and for evaluating modeling of atmospheric organics. We also develop an additional parameterization for models to estimate the ratio of primary OM to OC from simulated NOx concentrations. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Philip, S.; Martin, R. V.; Pierce, J. R.; Nowlan, C. R.; Cooper, M. J.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada.
[Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pierce, J. R.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Jimenez, J. L.] Univ Colorado, Dept Chem & Biochem, CIRES, Boulder, CO 80309 USA.
[Zhang, Q.] Univ Calif Davis, Dept Environm Toxicol, Davis, CA 95616 USA.
[Canagaratna, M. R.] Aerodyne Res Inc, Billerica, MA USA.
[Spracklen, D. V.] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England.
[Lamsal, L. N.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Lamsal, L. N.; Krotkov, N. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Philip, S (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada.
EM philip.sajeev@dal.ca
RI Pierce, Jeffrey/E-4681-2013; Jimenez, Jose/A-5294-2008; Zhang,
Qi/F-9653-2010; Martin, Randall/C-1205-2014; Krotkov,
Nickolay/E-1541-2012; Spracklen, Dominick/B-4890-2014;
OI Pierce, Jeffrey/0000-0002-4241-838X; Jimenez, Jose/0000-0001-6203-1847;
Martin, Randall/0000-0003-2632-8402; Krotkov,
Nickolay/0000-0001-6170-6750; Nowlan, Caroline/0000-0002-8718-9752
FU NSERC; DOE (BER/ASR) [DE SC0006035/DE-SC0006711/DE-FG02-11ER65293];
[DE-FG02-11ER65293]
FX This work was supported by NSERC. JLJ was supported by DOE (BER/ASR) DE
SC0006035/DE-SC0006711/DE-FG02-11ER65293. QZ was supported by
DE-FG02-11ER65293. We thank Aaron van Donkelaar and Ian Folkins for
useful comments.
NR 61
TC 11
Z9 12
U1 5
U2 26
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD APR
PY 2014
VL 87
BP 34
EP 40
DI 10.1016/j.atmosenv.2013.11.065
PG 7
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AY2QR
UT WOS:000347434900005
ER
PT J
AU Zhang, QG
Knapp, C
Smith, J
Evans, J
AF Zhang, Qingguang
Knapp, Charles
Smith, Jeffrey
Evans, Joyce
TI Cardiovascular responses to orthostatic stress after 90 minutes
head-down bed rest and artificial gravity exposure in hypovolemic men
and women
SO FASEB JOURNAL
LA English
DT Meeting Abstract
C1 [Smith, Jeffrey] NASA, Ames Res Ctr, Mountain View, CA USA.
[Zhang, Qingguang; Knapp, Charles; Evans, Joyce] Univ Kentucky, Dept Biomed Engn, Lexington, KY USA.
NR 0
TC 0
Z9 0
U1 1
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
EI 1530-6860
J9 FASEB J
JI Faseb J.
PD APR
PY 2014
VL 28
IS 1
SU S
MA 1169.18
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA AX0OG
UT WOS:000346651002256
ER
PT J
AU Sim, BW
JanakiRam, RD
Lau, BH
AF Sim, Ben W.
JanakiRam, Ram D.
Lau, Benton H.
TI Reduced In-Plane, Low-Frequency Noise of an Active Flap Rotor
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
AB Results from a joint DARPA/Boeing/NASA/Army wind tunnel test demonstrated the ability to reduce in-plane, low-frequency noise of the full-scale Boeing-SMART(Smart Material Actuated Rotor Technology) rotor with active flaps. Test data reported in this paper illustrated that near-field acoustic energy in the first six blade-passing harmonics could be reduced by up to 6 dB at a moderate-airspeed, level flight condition at an advance ratio of 0.30. Reduced noise levels were attributed to selective active flap schedules that modified in-plane blade airloads on the advancing side of the rotor, generating counteracting acoustic pulses that partially offset the negative pressure peaks associated with in-plane, steady thickness noise. These favorable reduced-noise operating states are a strong function of the active flap actuation amplitude, frequency, and phase. The reduced noise levels resulted in reduction of predicted aural detection distance, but incurred vibratory load penalties due to increased hub shear forces.
C1 [Sim, Ben W.] US Army Res Dev & Engn Command, AeroflightDynam Directorate, Moffett Field, CA 94035 USA.
[JanakiRam, Ram D.] Boeing Co, Flight Technol, Mesa, AZ USA.
[Lau, Benton H.] NASA, Aeromech Branch, Ames Res Ctr, Moffett Field, CA USA.
RP Sim, BW (reprint author), US Army Res Dev & Engn Command, AeroflightDynam Directorate, Moffett Field, CA 94035 USA.
EM ben.w.sim@us.army.mil
NR 20
TC 2
Z9 2
U1 0
U2 1
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
EI 2161-6027
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD APR
PY 2014
VL 59
IS 2
AR 022002
DI 10.4050/JAHS.59.022002
PG 17
WC Engineering, Aerospace
SC Engineering
GA AS6HW
UT WOS:000344365800002
ER
PT J
AU Isaacson, DR
Sadovsky, AV
Davis, D
AF Isaacson, D. R.
Sadovsky, A. V.
Davis, D.
TI Tactical Scheduling for Precision Air Traffic Operations: Past Research
and Current Problems
SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS
LA English
DT Article
ID LANDINGS
C1 [Isaacson, D. R.; Sadovsky, A. V.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Davis, D.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
RP Isaacson, DR (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM douglas.r.isaacson@nasa.gov
NR 57
TC 4
Z9 4
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 APR
PY 2014
VL 11
IS 4
BP 234
EP 256
DI 10.2514/1.I010119
PG 23
WC Engineering, Aerospace
SC Engineering
GA AP4RO
UT WOS:000342066200006
ER
PT J
AU Carney, LT
Reinsch, SS
Lane, PD
Solberg, OD
Jansen, LS
Williams, KP
Trent, JD
Lane, TW
AF Carney, Laura T.
Reinsch, Sigrid S.
Lane, Pamela D.
Solberg, Owen D.
Jansen, Lara S.
Williams, Kelly P.
Trent, Jonathan D.
Lane, Todd W.
TI Microbiome analysis of a microalgal mass culture growing in municipal
wastewater in a prototype OMEGA photobioreactor
SO ALGAL RESEARCH-BIOMASS BIOFUELS AND BIOPRODUCTS
LA English
DT Article
DE Photobioreactor; Microbiome; Second generation sequencing; Algal
pathogens; Biocontaminant
ID DIVERSITY; ALGAE; BACTERIA; GROWTH; RDNA; QUANTIFICATION;
IDENTIFICATION; ENVIRONMENT; ASSOCIATION; COMMUNITIES
AB Large-scale cultivation of microalgae for biofuels may avoid competing for agriculture, water, and fertilizer by using wastewater and avoid competing for land by using the Offshore Membrane Enclosures for Growing Algae (OMEGA) system. Some microalgae thrive in wastewater; however, wastewater also contains a complex mixture of organisms. An algae culture in wastewater from a San Francisco Treatment Facility in a 1600-L OMEGA culture system was monitored by standard methods. Prima facie evidence of a chytrid infection prompted a detailed investigation of the microbiome over a 13-day period using second generation sequencing of hypervariable regions of the small subunit rRNA genes. The observed bacteria, initially dominated by.-proteobacteria, shifted to Cytophagia, Flavobacteriia, and Sphingobacteriia after addition of exogenous nutrients. The dominant algae genera introduced with the inoculum, Desmodesmus and Scenedesmus, remained over 70% of the sequence reads on day 13, although the optical density and fluorescence of the culture declined. Nonalgal eukarya, initially dominated by unclassified alveolates, chrysophytes, and heliozoan grazers, shifted to chytrid fungi on day 5 and continued to day 13. The results of this microbiome analysis can facilitate the development of probe or primer based surveillance systems for routine monitoring of large-scale microalgae cultures. Published by Elsevier B.V.
C1 [Carney, Laura T.; Lane, Pamela D.; Solberg, Owen D.; Jansen, Lara S.; Williams, Kelly P.; Lane, Todd W.] Sandia Natl Labs, Livermore, CA 94551 USA.
[Reinsch, Sigrid S.; Trent, Jonathan D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lane, TW (reprint author), Sandia Natl Labs, POB 969,MS 9292, Livermore, CA 94551 USA.
EM twlane@sandia.gov
OI Lane, Todd/0000-0002-5816-2649
FU U.S. Department of Energy's National Nuclear Security Administration
[DE-AC04-94AL85000]; Biomass Program of the Office of Energy Efficiency
and Renewable Energy U.S. Department of Energy [NL0022897]; NASA;
California Energy Commission
FX Sandia National Laboratories is a multi-program laboratory managed and
operated by Sandia Corporation, a wholly owned subsidiary of Lockheed
Martin Corporation, for the U.S. Department of Energy's National Nuclear
Security Administration under contract DE-AC04-94AL85000. Microbiome
analysis carried out at Sandia National Laboratories was supported by
the Biomass Program of the Office of Energy Efficiency and Renewable
Energy U.S. Department of Energy under Award #NL0022897. We thank the
OMEGA team for technical support, especially Sasha Tozzi, John
Malinowski, Hiromi Kagawa, Tsegereda Embaye, Kit Clark, Linden Harris,
Patrick Wiley, John Rask, Rus Adams, Zach Hall and the staff at the San
Francisco Southeast Wastewater Treatment Plant. We acknowledge Heather
McDonald for editorial assistance. The OMEGA project was funded by NASA
and the California Energy Commission.
NR 64
TC 15
Z9 15
U1 4
U2 65
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 2211-9264
J9 ALGAL RES
JI Algal Res.
PD APR
PY 2014
VL 4
BP 52
EP 61
DI 10.1016/j.algal.2013.11.006
PG 10
WC Biotechnology & Applied Microbiology
SC Biotechnology & Applied Microbiology
GA AM6MP
UT WOS:000339979600008
ER
PT J
AU Stehlik, LL
Pessutti, J
Rosendale, J
Phelan, B
AF Stehlik, Linda L.
Pessutti, Jeff
Rosendale, John
Phelan, Beth
TI Residence time and habitat duration for predators in a small
mid-Atlantic estuary
SO FISHERY BULLETIN
LA English
DT Article
ID FLOUNDER PSEUDOPLEURONECTES-AMERICANUS; BLUEFISH POMATOMUS-SALTATRIX;
JUVENILE WINTER FLOUNDER; MIGRATORY STRIPED BASS; SOUTHERN NEW-JERSEY;
ACOUSTIC TELEMETRY; FISH RECRUITMENT; MORONE-SAXATILIS; EAST-COAST;
DYNAMICS
AB Residence times of individual fishes should reflect the durations over which habitat resources support survival, metabolic maintenance, and adequate growth. From May to October in 2006 and 2007, we measured residencies of ultrasonically tagged age-1+ Striped Bass (Morone saxatilis; n=46), age-0 and age-1+ Bluefish (Pomatomus saltatrix; n=45 and 35) and age-1+ Weakfish (Cynoscion regalis; n=41) in a small estuarine tributary in New Jersey with 32 ultrasonic receivers to monitor movements and sensors to measure habitat resources. Striped Bass and age-1+ Bluefish used the estuary for medians of 9.5 days (d) (max=58 d) and 22 d (max=88 d), and age-0 Bluefish and Weakfish were resident for medians of 30 d (max=52 d) and 41 d (max=88 d), respectively. Small individuals <500 mm TL were likely to remain in the estuary longer at warmer temperatures than were large individuals. Size-dependent temperature responses were similar to optimal temperatures for growth reported in previous studies. Freshwater discharge also influenced residence time. All species were likely to remain in the estuary until freshwater discharge rates fell to a value associated with the transition of the estuarine state from a partially to fully mixed state. This transition weakens flows into the upstream salt front where prey concentrations usually are high. Time of estuarine residence appeared to be regulated by temperatures that controlled scopes for growth and the indirect effects of freshwater discharge on prey productivity and concentration. Changes in the seasonal phenology of temperature, precipitation, and human water use could alter the durations over which small estuarine tributaries serve as suitable habitats.
C1 [Stehlik, Linda L.; Pessutti, Jeff; Rosendale, John; Phelan, Beth] NOAA, Behav Ecol Branch, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv,James J Howard Marine, Highlands, NJ 07732 USA.
RP Stehlik, LL (reprint author), NOAA, Behav Ecol Branch, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv,James J Howard Marine, 74 Magruder Rd, Highlands, NJ 07732 USA.
NR 57
TC 0
Z9 0
U1 3
U2 16
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
EI 1937-4518
J9 FISH B-NOAA
JI Fish. Bull.
PD APR-JUL
PY 2014
VL 112
IS 2-3
BP 144
EP 158
DI 10.7755/FB.112.2-3.4
PG 15
WC Fisheries
SC Fisheries
GA AM7XE
UT WOS:000340081200004
ER
PT J
AU Asami, F
Enoto, T
Iwakiri, W
Yamada, S
Tamagawa, T
Mihara, T
Nagase, F
AF Asami, Fumi
Enoto, Teruaki
Iwakiri, Wataru
Yamada, Shin'ya
Tamagawa, Toru
Mihara, Tatehiro
Nagase, Fumiaki
TI Broad-band spectroscopy of Hercules X-1 with Suzaku
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE binaries: spectroscopic; pulsars: individual (Hercules X-1); X-rays:
stars
ID X-RAY BINARIES; PULSE-PHASE; COMPTON REFLECTION; CYCLOTRON LINE; 35-DAY
CYCLE; X-1; SPECTRUM; BEPPOSAX; STATE; ABSORPTION
AB Hercules X-1 was observed with Suzaku in the main-on state from 2005 to 2010. The 0.4-100 keV wide-band spectra obtained in four observations showed a broad hump around 4-9 keV in addition to narrow Fe lines at 6.4 and 6.7 keV. The hump was seen in all the four observations regardless of the selection of the continuum models. Thus it is considered a stable and intrinsic spectral feature in Her X-1. The broad hump lacked a sharp structure like an absorption edge. Thus it was represented by two different spectral models: an ionized partial covering or an additional broad line at 6.5 keV. The former required a persistently existing ionized absorber, whose origin was unclear. In the latter case, the Gaussian fitting of the 6.5-keV line needs a large width of sigma = 1.0-1.5 keV and a large equivalent width of 400-900 eV. If the broad line originates from Fe fluorescence of accreting matter, its large width may be explained by the Doppler broadening in the accretion flow. However, the large equivalent width may be inconsistent with a simple accretion geometry.
C1 [Asami, Fumi; Enoto, Teruaki; Iwakiri, Wataru; Yamada, Shin'ya; Tamagawa, Toru] RIKEN, Nishina Ctr, Wako, Saitama 3510198, Japan.
[Asami, Fumi; Tamagawa, Toru] Tokyo Univ Sci, Dept Phys, Shinjuku Ku, Tokyo 1628601, Japan.
[Enoto, Teruaki] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mihara, Tatehiro] RIKEN, MAXI Team, Wako, Saitama 3510198, Japan.
[Nagase, Fumiaki] Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2298510, Japan.
RP Asami, F (reprint author), RIKEN, Nishina Ctr, 2-1 Hirosawa, Wako, Saitama 3510198, Japan.
EM asami@crab.riken.jp
RI XRAY, SUZAKU/A-1808-2009; Mihara, Tatehiro/C-5536-2017
OI Mihara, Tatehiro/0000-0002-6337-7943
FU JSPS Fellows
FX This work was supported by a Grant-in-Aid for JSPS Fellows.
NR 32
TC 1
Z9 1
U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD APR
PY 2014
VL 66
IS 2
AR 44
DI 10.1093/pasj/psu005
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8YZ
UT WOS:000339427200006
ER
PT J
AU Sasano, M
Makishima, K
Sakurai, S
Zhang, Z
Enoto, T
AF Sasano, Makoto
Makishima, Kazuo
Sakurai, Soki
Zhang, Zhongli
Enoto, Teruaki
TI Suzaku view of the neutron star in the dipping source 4U 1822-37
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE accretion, accretion disks; stars: magnetic fields; X-rays: binaries
ID X-RAY BINARIES; ACCRETION DISK; BOARD SUZAKU; SOURCE X1822-371;
MAGNETIC-FIELDS; ORBITAL-PERIOD; EMISSION-LINES; SPIN PERIOD;
SPECTROSCOPY; PULSARS
AB The dipping X-ray source 4U 1822-37 was observed by Suzaku on 2006 October 20 for a net exposure of 37 ks. The source was detected with the XIS at a 1-10 keV flux of 5.5 x 10(-10) erg cm(-2) s(-1), and with the HXD (HXD-PIN) at a 10-50 keV flux of 8.9 x 10(-10) erg cm(-2) s(-1). With HXD-PIN, the pulsation was detected at a barycentric period of 0.592437 s, and its change rate was reconfirmed as -2.43 x 10(-12) s s(-1). The 1-50 keV spectra of 4U 1822-37 were found to be very similar to those of Her X-1 in the slopes, cutoff, and iron lines. Three iron lines (Fe K alpha, Fe XXV, and Fe XXVI) were detected, on top of a 1-50 keV continuum that is described by an NPEX model plus a soft blackbody. In addition, a cyclotron resonance scattering feature was detected significantly (> 99% confidence), at an energy of 33 +/- 2 keV with a depth of 0.4(-0.3)(+0.6). Therefore, the neutron star in this source is concluded to have a strong magnetic field of 2.8 x 10(12) G. Further assuming that the source has a relatively high intrinsic luminosity of several times 10(37) erg s(-1), its spectral and timing properties are consistently explained.
C1 [Sasano, Makoto; Makishima, Kazuo; Sakurai, Soki; Zhang, Zhongli] Univ Tokyo, Sch Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Makishima, Kazuo; Enoto, Teruaki] RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan.
[Makishima, Kazuo] Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan.
[Enoto, Teruaki] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Sasano, M (reprint author), Univ Tokyo, Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
EM sasano@juno.phys.s.u-tokyo.ac.jp
RI XRAY, SUZAKU/A-1808-2009
FU JSPS [23244024, 24-3320]
FX We thank all members of the Suzaku hardware and software teams and the
Science Working Group. M. S., K. M., and T. E. are supported by the
Japan Society for the Promotion of Science (JSPS) Research Fellowship
for Young Scientists, Grant-in-Aid for Scientific Research (A)
(23244024) from JSPS, and Grant-in-Aid for JSPS Fellows, 24-3320,
respectively.
NR 40
TC 7
Z9 7
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD APR
PY 2014
VL 66
IS 2
AR 35
DI 10.1093/pasj/psu002
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8YZ
UT WOS:000339427200003
ER
PT J
AU Frazer, RE
Coleman, DS
Mills, RD
AF Frazer, Ryan E.
Coleman, Drew S.
Mills, Ryan D.
TI Zircon U-Pb geochronology of the Mount Givens Granodiorite: Implications
for the genesis of large volumes of eruptible magma
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID CENTRAL SIERRA-NEVADA; FISH CANYON MAGMA; JUAN VOLCANIC FIELD; TUFF
AEGEAN ARC; NEW-ZEALAND; AR-40/AR-39 CHRONOLOGY; PLUTON EMPLACEMENT;
ADAMELLO BATHOLITH; CALDERA COMPLEX; INTRUSIVE SUITE
AB The Mount Givens Granodiorite, a large pluton in the central Sierra Nevada batholith, California, is similar in area to zoned intrusive suites yet is comparatively chemically and texturally homogenous. New zircon U-Pb geochronology indicates that the pluton was constructed over at least 7 Ma from 97.92 +/- 0.06 Ma to 90.87 +/- 0.05 Ma. Combining the new geochronology with the exposed volume of the pluton yields an estimated magma flux of <0.001 km(3)/a. The geochronologic data are at odds with the previously speculated links between plutons such as the Mount Givens Granodiorite and large-volume homogeneous ignimbrites (often termed monotonous intermediates). Existing data indicate that large plutons accumulate at rates of <= 0.001 km(3)/a, 1-2 orders of magnitude less than fluxes calculated for dated monotonous intermediates. If monotonous intermediates are remobilized, erupted plutons accumulated at rates comparable to dated examples, they should preserve a record of zircon growth of up to 10 Ma. Alternatively, the long history of zircon growth recorded in plutons may be erased during the processes of reheating and remobilization that precede supervolcano eruption. However, zircon dissolution modeling, based on hypothetical temperature-time histories for preeruptive monotonous intermediates, indicates that rejuvenation events would not sufficiently dissolve zircon. We suggest that eruptions of monotonous intermediates occur during high magmatic flux events, leaving little behind in the intrusive rock record, whereas low fluxes favor pluton accumulation.
C1 [Frazer, Ryan E.; Coleman, Drew S.] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27514 USA.
[Mills, Ryan D.] NASA JSC, Astromat Res & Explorat Sci Directorate, Houston, TX USA.
RP Frazer, RE (reprint author), Univ N Carolina, Dept Geol Sci, Mitchell Hall, Chapel Hill, NC 27514 USA.
EM ryan.frazer@unc.edu
FU UNC Department of Geological Sciences Martin Fund; Sigma Xi; Geological
Society of America
FX Frazer was supported by grants from the UNC Department of Geological
Sciences Martin Fund, Sigma Xi, and the Geological Society of America.
Courtney Beck and Daniel Gurganus provided field assistance, and Jeremy
Inglis and Miquela Ingalls gave useful laboratory aid. Informal reviews
by Allen Glazner and Kevin Stewart on an earlier version of the
manuscript helped refine the ideas presented here. We thank Bruce Watson
for discussions about zircon dissolution. Editor Michael Walter,
Catherine Annen, and an anonymous reviewer provided comments that led to
a much stronger presentation.
NR 108
TC 12
Z9 12
U1 1
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD APR
PY 2014
VL 119
IS 4
BP 2907
EP 2924
DI 10.1002/2013JB010716
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AJ4ZG
UT WOS:000337688600018
ER
PT J
AU Chambon, P
Zhang, SQ
Hou, AY
Zupanski, M
Cheung, S
AF Chambon, Philippe
Zhang, Sara Q.
Hou, Arthur Y.
Zupanski, Milija
Cheung, Samson
TI Assessing the impact of pre-GPM microwave precipitation observations in
the Goddard WRF ensemble data assimilation system
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE precipitation; ensemble data assimilation; microwave observations;
forecasts verification; Global Precipitation Measurement Mission
ID RADAR RAINFALL PRODUCT; CLOUD-RESOLVING MODEL; VARIATIONAL ASSIMILATION;
KALMAN FILTER; PART I; RADIANCES; FORECASTS; SCHEME; IMAGER; RATES
AB The forthcoming Global Precipitation Measurement (GPM) Mission will provide next-generation precipitation observations from a constellation of satellites. Since precipitation by nature has large variability and low predictability at cloud-resolving scales, the impact of precipitation data on the skills of mesoscale numerical weather prediction (NWP) is largely affected by the characterization of background and observation errors and the representation of nonlinear cloud/precipitation physics in an NWP data assimilation system.
We present a data impact study on the assimilation of precipitation-affected microwave (MW) radiances from a pre-GPM satellite constellation using the Goddard WRF Ensemble Data Assimilation System (Goddard WRF-EDAS). A series of assimilation experiments are carried out in a Weather Research Forecast (WRF) model domain of 9 km resolution in western Europe. Sensitivities to observation error specifications, background error covariance estimated from ensemble forecasts with different ensemble sizes, and MW channel selections are examined through single-observation assimilation experiments. An empirical bias correction for precipitation-affected MW radiances is developed based on the statistics of radiance innovations in rainy areas. The data impact is assessed by full data assimilation cycling experiments for a storm event that occurred in France in September 2010. Results show that the assimilation of MW precipitation observations from a satellite constellation mimicking GPM has a positive impact on the accumulated rain forecasts verified with surface radar rain estimates. The case-study on a convective storm also reveals that the accuracy of ensemble-based background error covariance is limited by sampling errors and model errors such as precipitation displacement and unresolved convective scale instability.
C1 [Chambon, Philippe] Univ Space Res Assoc, Columbia, MD USA.
[Chambon, Philippe; Zhang, Sara Q.; Hou, Arthur Y.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
[Zupanski, Milija] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Cheung, Samson] Univ Calif Davis, Dept Math, Davis, CA 95616 USA.
RP Zhang, SQ (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM sara.q.zhang@nasa.gov
RI Measurement, Global/C-4698-2015
FU Global precipitation Measurement (GPM) Flight Project at NASA Goddard
Space Flight Center; French Ministry of the environment
FX The authors thank Wesley Berg at Colorado State University for providing
the SSMIS FCDR inter-calibrated brightness temperature dataset, and
Meteo-France and HyMex database teams (ESPRI/IPSL, SEDOO/OMP) for
providing the surface rainfall product from the ARAMIS radar network.
Jean-Francois Mahfouf and Chris Kidd are acknowledged for their helpful
remarks. Jan Angevine is recognized for editing the manuscript. The
authors are grateful to two anonymous reviewers for their insightful and
constructive comments that improved the article. This research is
supported by the Global precipitation Measurement (GPM) Flight Project
at NASA Goddard Space Flight Center and the French Ministry of the
environment. Computations were performed at NASA Advanced Supercomputing
(NAS).
NR 50
TC 3
Z9 3
U1 4
U2 12
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2014
VL 140
IS 681
BP 1219
EP 1235
DI 10.1002/qj.2215
PN B
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AJ4ED
UT WOS:000337623500008
ER
PT J
AU Holdaway, D
Errico, R
AF Holdaway, D.
Errico, R.
TI Using Jacobian sensitivities to assess a linearization of the relaxed
Arakawa-Schubert convection scheme
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE adjoint; tangent linear; convection; 4D-Var; sensitivity; principle
components; parametrization
ID 4-DIMENSIONAL VARIATIONAL ASSIMILATION; MOIST PHYSICS SCHEMES;
OPERATIONAL IMPLEMENTATION; ADJOINT SENSITIVITY; INITIAL CONDITIONS;
OBSERVATION IMPACT; PROGNOSTIC CLOUD; MESOSCALE MODEL; ECMWF MODEL;
PRECIPITATION
AB The inclusion of linearized moist physics can increase the accuracy of 4D-Var data assimilation and adjoint-based sensitivity analysis. Moist processes such as convection can exhibit nonlinear behaviour. As a result, representation of these processes in a linear way requires much care; a straightforward linearization may yield a poor approximation to the behaviour of perturbations of interest and could contain numerical instability. Here, an extensive numerical study of the Jacobian of the relaxed Arakawa-Schubert (RAS) convection scheme is shown. A Jacobian based on perturbations at individual model levels can be used to understand the physical behaviour of the RAS scheme, predict how sensitive that behaviour is to the prognostic variables and determine the stability of a linearization of the scheme. The linearity of the scheme is also considered by making structured perturbations, constructed from the principle components of the model variables. Based on the behaviour of the Jacobian operator and the results when using structured perturbations, a suitable method for linearizing the RAS scheme is determined. For deep, strong convection, the structures of the RAS Jacobian are reasonably simple, the rate at which finite-amplitude estimates of the structures change with respect to input perturbations is small and the eigenmodes of the Jacobian are not prohibitively unstable. For deep convection, an exact linearization is therefore suitable. For shallow convection, the RAS scheme can be more sensitive to the input prognostic variables due to the faster time-scales and proximity to switches. Linearization of the RAS therefore requires some simplifications to smooth the behaviour for shallow convection. It is noted that the physical understanding of the scheme gained from examining the Jacobian provides a useful tool to the developers of nonlinear physical parametrizations.
C1 [Holdaway, D.; Errico, R.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Holdaway, D.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Greenbelt, MD USA.
[Errico, R.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD USA.
RP Holdaway, D (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM dan.holdaway@nasa.gov
RI Holdaway, Daniel/Q-5198-2016
OI Holdaway, Daniel/0000-0002-3672-2588
NR 38
TC 2
Z9 2
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2014
VL 140
IS 681
BP 1319
EP 1332
DI 10.1002/qj.2210
PN B
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AJ4ED
UT WOS:000337623500017
ER
PT J
AU Igel, MR
van den Heever, SC
Stephens, GL
Posselt, DJ
AF Igel, Matthew R.
van den Heever, Susan C.
Stephens, Graeme L.
Posselt, Derek J.
TI Convective-scale responses of a large-domain, modelled tropical
environment to surface warming
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE convection; climate; cloud-resolving models
ID CLOUD-RESOLVING MODEL; WATER-VAPOR; TROPOSPHERIC HUMIDITY; EXTREME
PRECIPITATION; HYDROLOGICAL CYCLE; MOISTURE-CONTENT; DEEP CONVECTION;
SIMULATIONS; CLIMATE; TRENDS
AB This article explores the response of convective-scale atmospheric characteristics to surface temperature through the lens of large-domain, cloud-system-resolving model experiments run at radiative convective equilibrium. We note several features reminiscent of the response to surface warming in atmospheric general circulation models. These include an increase in the rain rate that is smaller than the modelled increase in precipitable water, a systematic decrease in sensible heating and an increase in clear-sky cooling. However, in contrast to climate models, we note that tropospheric relative humidity increases and column-integrated water vapour increases at the rate anticipated from the Clausius-Clapeyron relationship, but only when compared with the troposphere mean temperature rather than surface temperature. Also shown are results elucidating the changes in the vertically integrated water budget and the distribution of high precipitation rates shifting toward higher rates. Moist static energy distributions are analyzed and, from these, clouds are implicated in effecting the final equilibrium state of the atmosphere. The results indicate that, while there are aspects of the tropical equilibrium that are represented realistically in current general circulation model climate-change experiments, there are potentially influential local interactions that are sufficiently important as to alter the mean response of the tropical water and energy balance to changes in sea-surface temperature. Convection is shown to dictate the equilibrium state across all scales, including those unresolved in climate models, rather than only responding to surface-induced changes.
C1 [Igel, Matthew R.; van den Heever, Susan C.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Posselt, Derek J.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Igel, MR (reprint author), Colorado State Univ, Dept Atmospher Sci, 1371 Campus Delivery, Ft Collins, CO 80523 USA.
EM MattIgel@atmos.colostate.edu
RI Igel, Matthew/A-5727-2013; van den Heever, Susan/E-8728-2011; Posselt,
Derek/I-4912-2012
OI Igel, Matthew/0000-0001-8916-544X; van den Heever,
Susan/0000-0001-9843-3864; Posselt, Derek/0000-0002-5670-5822
FU NASA CloudSat grant [5-319160]; NASA [49683]; NASA Modelling, Analysis,
and Prediction grant [NNX09AJ43G]
FX This work was supported by NASA CloudSat grant 5-319160. S. van den
Heever was supported by NASA grant 49683. A. D. Posselt was supported by
NASA Modelling, Analysis, and Prediction grant NNX09AJ43G. The authors
thank two anonymous reviewers who helped to make this document more
precise.
NR 60
TC 1
Z9 1
U1 0
U2 10
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2014
VL 140
IS 681
BP 1333
EP 1343
DI 10.1002/qj.2230
PN B
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AJ4ED
UT WOS:000337623500018
ER
PT J
AU Baker, WE
Atlas, R
Cardinali, C
Clement, A
Emmitt, GD
Gentry, BM
Hardesty, RM
Kallen, E
Kavaya, MJ
Langland, R
Ma, ZZ
Masutani, M
McCarty, W
Pierce, RB
Pu, ZX
Riishojgaard, LP
Ryan, J
Tucker, S
Weissmann, M
Yoe, JG
AF Baker, Wayman E.
Atlas, Robert
Cardinali, Carla
Clement, Amy
Emmitt, George D.
Gentry, Bruce M.
Hardesty, R. Michael
Kaellen, Erland
Kavaya, Michael J.
Langland, Rolf
Ma, Zaizhong
Masutani, Michiko
McCarty, Will
Pierce, R. Bradley
Pu, Zhaoxia
Riishojgaard, Lars Peter
Ryan, James
Tucker, Sara
Weissmann, Martin
Yoe, James G.
TI LIDAR-MEASURED WIND PROFILES The Missing Link in the Global Observing
System
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID DATA ASSIMILATION SYSTEM; VARIATIONAL DATA ASSIMILATION; INCOHERENT
DOPPLER LIDAR; OBSERVATION IMPACT; AIRBORNE DEMONSTRATOR; SPECTRAL
ANALYZER; ERA-40 REANALYSIS; MIDDLE ATMOSPHERE; EDGE TECHNIQUE;
SOLID-STATE
C1 [Baker, Wayman E.] NOAA, Mchenry, MD USA.
[Atlas, Robert] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA.
[Cardinali, Carla; Kaellen, Erland] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[Clement, Amy] Univ Miami, Miami, FL USA.
[Emmitt, George D.] Simpson Weather Associates, Charlottesville, VA USA.
[Gentry, Bruce M.; McCarty, Will] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Hardesty, R. Michael] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Kavaya, Michael J.] NASA Langley Res Ctr, Hampton, VA USA.
[Langland, Rolf] Naval Res Lab, Monterey, CA USA.
[Riishojgaard, Lars Peter] World Meteorol Org, Geneva, Switzerland.
[Ma, Zaizhong; Yoe, James G.] Joint Ctr Satellite Data Assimilat, College Pk, MD USA.
[Masutani, Michiko] NOAA, Environm Modeling Ctr, College Pk, MD USA.
[Pierce, R. Bradley] NOAA, Natl Environm Satellite Data & Informat Serv, Madison, WI USA.
[Pu, Zhaoxia] Univ Utah, Salt Lake City, UT USA.
[Ryan, James] Univ New Hampshire, Durham, NH 03824 USA.
[Tucker, Sara] Ball Aerosp & Technol Corp, Boulder, CO USA.
[Weissmann, Martin] Univ Munich, Hans Ertel Ctr Weather Res, Munich, Germany.
RP Baker, WE (reprint author), 253 Gleanings Dr, Mchenry, MD 21541 USA.
EM wayman.baker@gmail.com
RI Weissmann, Martin/C-9084-2013; Pierce, Robert Bradley/F-5609-2010;
Atlas, Robert/A-5963-2011; Manager, CSD Publications/B-2789-2015
OI Pierce, Robert Bradley/0000-0002-2767-1643; Atlas,
Robert/0000-0002-0706-3560;
FU Earth Science Division at NASA headquarters; NASA Earth Science
Technology Office at the Goddard Space Flight Center; SWA; German
Federal Ministry of Transport, Building and Urban Development
FX The authors thank Dr. Ramesh Kakar of the Earth Science Division at NASA
headquarters and Dr. George Komar of the NASA Earth Science Technology
Office at the Goddard Space Flight Center for supporting research with
DWL data, including airborne campaigns, and funding hardware risk
reduction studies to advance the readiness of the DWL technology for
space. The authors thank Dr. John Cortinas and NOAA's Office of Weather
and Air Quality for contributing to the support for DWL OSSEs through
NOAA's OSSE Testbed. The expert assistance of Paul Berrisford of ECMWF
is sincerely acknowledged. Sidney Wood and Steven Greco of Simpson
Weather Associates (SWA) are acknowledged for their dedication to
producing simulated space-based DWL observations used in the OSSEs and
processing and analyzing data from the U.S. Navy's airborne DWL. Funding
for manuscript preparation and submission was provided by SWA. M.
Weissmann is part of the Hans-Ertel Centre for Weather Research, a
network of universities, research institutes, and Deutscher Wetterdienst
funded by the German Federal Ministry of Transport, Building and Urban
Development.
NR 131
TC 24
Z9 25
U1 3
U2 24
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 APR
PY 2014
VL 95
IS 4
BP 543
EP 564
DI 10.1175/BAMS-D-12-00164.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AI8MK
UT WOS:000337170300006
ER
PT J
AU Kirtman, BP
Min, D
Infanti, JM
Kinter, JL
Paolino, DA
Zhang, Q
van den Dool, H
Saha, S
Mendez, MP
Becker, E
Peng, PT
Tripp, P
Huang, J
DeWitt, DG
Tippett, MK
Barnston, AG
Li, SH
Rosati, A
Schubert, SD
Rienecker, M
Suarez, M
Li, ZE
Marshak, J
Lim, YK
Tribbia, J
Pegion, K
Merryfield, WJ
Denis, B
Wood, EF
AF Kirtman, Ben P.
Min, Dughong
Infanti, Johnna M.
Kinter, James L., III
Paolino, Daniel A.
Zhang, Qin
van den Dool, Huug
Saha, Suranjana
Mendez, Malaquias Pena
Becker, Emily
Peng, Peitao
Tripp, Patrick
Huang, Jin
DeWitt, David G.
Tippett, Michael K.
Barnston, Anthony G.
Li, Shuhua
Rosati, Anthony
Schubert, Siegfried D.
Rienecker, Michele
Suarez, Max
Li, Zhao E.
Marshak, Jelena
Lim, Young-Kwon
Tribbia, Joseph
Pegion, Kathleen
Merryfield, William J.
Denis, Bertrand
Wood, Eric F.
TI THE NORTH AMERICAN MULTIMODEL ENSEMBLE Phase-1 Seasonal-to-Interannual
Prediction; Phase-2 toward Developing Intraseasonal Prediction
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID DATA ASSIMILATION SYSTEM; UNITED-STATES; FORECAST SYSTEM; ENSO
PREDICTION; CLIMATE; MODEL; IMPACT; SKILL; PROBABILITY; CALIBRATION
C1 [Kirtman, Ben P.; Min, Dughong; Infanti, Johnna M.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA.
[Kinter, James L., III; Paolino, Daniel A.] Ctr Ocean Land Atmosphere Studies, Calverton, MD USA.
[Zhang, Qin; van den Dool, Huug; Saha, Suranjana; Mendez, Malaquias Pena; Becker, Emily; Peng, Peitao; Tripp, Patrick; Huang, Jin] NOAA, Natl Ctr Environm Predict, Camp Springs, MD USA.
[DeWitt, David G.; Tippett, Michael K.; Barnston, Anthony G.; Li, Shuhua] Int Res Inst Climate & Soc, Palisades, NY USA.
[Tippett, Michael K.] King Abdulaziz Univ, Dept Meteorol, Ctr Excellence Climate Change Res, Jeddah 21413, Saudi Arabia.
[Rosati, Anthony] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Schubert, Siegfried D.; Rienecker, Michele; Suarez, Max; Li, Zhao E.; Marshak, Jelena; Lim, Young-Kwon] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Tribbia, Joseph] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Pegion, Kathleen] Univ Colorado, CIRES, Boulder, CO 80309 USA.
[Merryfield, William J.; Denis, Bertrand] Environm Canada, Fredericton, NB, Canada.
[Wood, Eric F.] Princeton Univ, Princeton, NJ 08544 USA.
RP Kirtman, BP (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA.
EM bkirtman@rsmas.miami.edu
RI Tippett, Michael/C-6286-2011
OI Tippett, Michael/0000-0002-7790-5364
FU NOAA MAPP program; NOAA MAPP; NSF; NASA; DOE
FX The phase-1 NMME project was supported by the NOAA MAPP program, and the
phase-2 NMME project is support by NOAA MAPP, NSF, NASA, and the DOE.
NR 34
TC 98
Z9 98
U1 3
U2 34
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 APR
PY 2014
VL 95
IS 4
BP 585
EP 601
DI 10.1175/BAMS-D-12-00050.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AI8MK
UT WOS:000337170300009
ER
PT J
AU Lin, HW
McCarty, JL
Wang, DD
Rogers, BM
Morton, DC
Collatz, GJ
Jin, YF
Randerson, JT
AF Lin, Hsiao-Wen
McCarty, Jessica L.
Wang, Dongdong
Rogers, Brendan M.
Morton, Douglas C.
Collatz, G. James
Jin, Yufang
Randerson, James T.
TI Management and climate contributions to satellite-derived active fire
trends in the contiguous United States
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
DE agriculture; air quality; carbon cycle; wildfire; aerosols
ID IMAGING SPECTRORADIOMETER MODIS; BURNED AREA; FOREST-FIRES; WILDFIRE;
NORTH; VALIDATION; ALGORITHMS; WEATHER; EMISSIONS; INCREASE
AB Fires in croplands, plantations, and rangelands contribute significantly to fire emissions in the United States, yet are often overshadowed by wildland fires in efforts to develop inventories or estimate responses to climate change. Here we quantified decadal trends, interannual variability, and seasonality of Terra Moderate Resolution Imaging Spectroradiometer (MODIS) observations of active fires (thermal anomalies) as a function of management type in the contiguous U.S. during 2001-2010. We used the Monitoring Trends in Burn Severity database to identify active fires within the perimeter of large wildland fires and land cover maps to identify active fires in croplands. A third class of fires defined as prescribed/other included all residual satellite active fire detections. Large wildland fires were the most variable of all three fire types and had no significant annual trend in the contiguous U.S. during 2001-2010. Active fires in croplands, in contrast, increased at a rate of 3.4% per year. Cropland and prescribed/other fire types combined were responsible for 77% of the total active fire detections within the U.S and were most abundant in the south and southeast. In the west, cropland active fires decreased at a rate of 5.9% per year, likely in response to intensive air quality policies. Potential evaporation was a dominant regulator of the interannual variability of large wildland fires, but had a weaker influence on the other two fire types. Our analysis suggests it may be possible to modify landscape fire emissions within the U.S. by influencing the way fires are used in managed ecosystems.
C1 [Lin, Hsiao-Wen; Rogers, Brendan M.; Jin, Yufang; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[McCarty, Jessica L.] Michigan Tech Res Inst, Ann Arbor, MI USA.
[Wang, Dongdong] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Morton, Douglas C.; Collatz, G. James] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
RP Lin, HW (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM hwlin@uci.edu
RI Wang, Dongdong/M-1969-2014; collatz, george/D-5381-2012; Morton,
Douglas/D-5044-2012
OI Wang, Dongdong/0000-0002-2076-576X;
FU NASA [NNX08AR69G, NNX10AL14G, NNX11AF96G]; Taiwan Merit Fellowship
[TMF-94-1A-016]
FX This research was funded by NASA grants NNX08AR69G and NNX10AL14G to Jin
and NNX11AF96G to Randerson. Lin received support from Taiwan Merit
Fellowship (TMF-94-1A-016). The audience may access the data in this
paper via contacting the authors.
NR 72
TC 5
Z9 5
U1 3
U2 25
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-8953
EI 2169-8961
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD APR
PY 2014
VL 119
IS 4
BP 645
EP 660
DI 10.1002/2013JG002382
PG 16
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA AI9UN
UT WOS:000337285500011
ER
PT J
AU Komendera, E
Reishus, D
Dorsey, JT
Doggett, WR
Correll, N
AF Komendera, Erik
Reishus, Dustin
Dorsey, John T.
Doggett, William R.
Correll, Nikolaus
TI Precise truss assembly using commodity parts and low precision welding
SO INTELLIGENT SERVICE ROBOTICS
LA English
DT Article
DE Robotic assembly; Autonomous robots; Precision manipulation; Space
robotics; Distributed robots
AB Hardware and software design and system integration for an intelligent precision jigging robot (IPJR), which allows high precision assembly using commodity parts and low-precision bonding, is described. Preliminary 2D experiments that aremotivated by the problem of assembling space telescope optical benches and very large manipulators on orbit using inexpensive, stock hardware and low-precision welding are also described. An IPJR is a robot that acts as the precise "jigging", holding parts of a local structure assembly site in place, while an external low precision assembly agent cuts and welds members. The prototype presented in this paper allows an assembly agent (for this prototype, a human using only low precision tools), to assemble a 2D truss made of wooden dowels to a precision on the order of millimeters over a span on the order of meters. The analysis of the assembly error and the results of building a square structure and a ring structure are discussed. Options for future work, to extend the IPJR paradigm to building in 3D structures at micron precision are also summarized.
C1 [Komendera, Erik; Reishus, Dustin; Correll, Nikolaus] Univ Colorado, Dept Comp Sci, Boulder, CO 80309 USA.
[Dorsey, John T.; Doggett, William R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Komendera, E (reprint author), Univ Colorado, Dept Comp Sci, Boulder, CO 80309 USA.
EM erik.komendera@colorado.edu; dustin.reishus@colorado.edu;
john.t.dorsey@nasa.gov; bill.doggett@nasa.gov;
nikolaus.correll@colorado.edu
FU NASA Office of the Chief Technologist's Space Technology Research
Fellowship
FX This work was supported by a NASA Office of the Chief Technologist's
Space Technology Research Fellowship.
NR 17
TC 2
Z9 2
U1 1
U2 9
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1861-2776
EI 1861-2784
J9 INTEL SERV ROBOT
JI Intell. Serv. Robot.
PD APR
PY 2014
VL 7
IS 2
SI SI
BP 93
EP 102
DI 10.1007/s11370-013-0144-4
PG 10
WC Robotics
SC Robotics
GA AI4QN
UT WOS:000336850000005
ER
PT J
AU Sun-Mack, S
Minnis, P
Chen, Y
Kato, S
Yi, YH
Gibson, SC
Heck, PW
Winker, DM
AF Sun-Mack, Sunny
Minnis, Patrick
Chen, Yan
Kato, Seiji
Yi, Yuhong
Gibson, Sharon C.
Heck, Patrick W.
Winker, David M.
TI Regional Apparent Boundary Layer Lapse Rates Determined from CALIPSO and
MODIS Data for Cloud-Height Determination
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID A-TRAIN; SATELLITE
AB Reliably determining low-cloud heights using a cloud-top temperature from satellite infrared imagery is often challenging because of difficulties in characterizing the local thermal structure of the lower troposphere with the necessary precision and accuracy. To improve low-cloud-top height estimates over water surfaces, various methods have employed lapse rates anchored to the sea surface temperature to replace the boundary layer temperature profiles that relate temperature to altitude. To further improve low-cloud-top height retrievals, collocated Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) and Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) data taken from July 2006 to June 2007 and from June 2009 to May 2010 (2 yr) for single-layer low clouds are used here with numerical weather model analyses to develop regional mean boundary apparent lapse rates. These parameters are designated as apparent lapse rates because they are defined using the cloud-top temperatures from satellite retrievals and surface skin temperatures; they do not represent true lapse rates. Separate day and night, seasonal mean lapse rates are determined for 100-resolution snow-free land, water, and coastal regions, while zonally dependent lapse rates are developed for snow/ice-covered areas for use in the Clouds and the Earth's Radiant Energy System (CERES) Edition 4 cloud property retrieval system (CCPRS-4). The derived apparent lapse rates over ice-free water range from 5 to 9K km(-1) with mean values of about 6.9 and 7.2K km(-1) during the day and night, respectively. Over land, the regional values vary from 3 to 8K km(-1), with day and night means of 5.5 and 6.2K km(-1), respectively. The zonal-mean apparent lapse rates over snow and ice surfaces generally decrease with increasing latitude, ranging from 4 to 8K km(-1). All of the CCPRS-4 lapse rates were used along with five other lapse rate techniques to retrieve cloud-top heights for 2 months of independent Aqua MODIS data. When compared with coincident CALIPSO data for October 2007, the mean cloud-top height differences between CCPRS-4 and CALIPSO during the daytime (nighttime) are 0.04 +/- 0.61 km(0.10 +/- 0.62 km) over ice-free water, 20.06 +/- 0.85 km(-0.01 +/- 0.83 km) over snow-free land, and 0.38 +/- 0.95km (0.03 +/- 0.92 km) over snow-covered areas. The CCPRS-4 regional monthly means are generally unbiased and lack spatial error gradients seen in the comparisons for most of the other techniques. Over snow-free land, the regional monthly-mean errors range from -0.28 +/- 0.74 km during daytime to 0.04 +/- 0.78 km at night. The water regional monthly means are, on average, 0.04 +/- 0.44 km less than the CALIPSO values during day and night. Greater errors are realized for snow-covered regions. Overall, the CCPRS-4 lapse rates yield the smallest RMS differences for all times of day over all areas both for individual retrievals and monthly means. These new regional apparent lapse rates, used in processing CERES Edition 4 data, should provide more accurate low-cloud-type heights than previously possible using satellite imager data.
C1 [Sun-Mack, Sunny; Chen, Yan; Yi, Yuhong; Gibson, Sharon C.] SSAI, Hampton, VA 23666 USA.
[Minnis, Patrick; Kato, Seiji; Winker, David M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Heck, Patrick W.] Univ Wisconsin, Cooperat Inst Meteorol Satellite Studies, Madison, WI USA.
RP Sun-Mack, S (reprint author), SSAI, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA.
EM szedung.sun-mack-1@nasa.gov
RI Minnis, Patrick/G-1902-2010
OI Minnis, Patrick/0000-0002-4733-6148
FU NASA CERES Project
FX Thanks are given to the three anonymous reviewers for their helpful
comments. This research was supported by the NASA CERES Project. The
CCCM data were obtained at
http://ceres.larc.nasa.gov/compare_products-ed2.php. The GOES and Rapid
Refresh analyses were acquired at the NASA Langley Satellite Imagery and
Cloud Products Page: http://cloudsgate2.larc.nasa.gov/index.html.
NR 33
TC 10
Z9 10
U1 2
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD APR
PY 2014
VL 53
IS 4
BP 990
EP 1011
DI 10.1175/JAMC-D-13-081.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AH9GG
UT WOS:000336449300013
ER
PT J
AU Kratz, DP
Stackhouse, PW
Gupta, SK
Wilber, AC
Sawaengphokhai, P
McGarragh, GR
AF Kratz, David P.
Stackhouse, Paul W., Jr.
Gupta, Shashi K.
Wilber, Anne C.
Sawaengphokhai, Parnchai
McGarragh, Greg R.
TI The Fast Longwave and Shortwave Flux (FLASHFlux) Data Product:
Single-Scanner Footprint Fluxes
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID ANGULAR-DISTRIBUTION MODELS; SYNCHRONOUS SATELLITE DATA; ENERGY SYSTEM
INSTRUMENT; SURFACE RADIATION; SOLAR-RADIATION; TERRA SATELLITE; ANNUAL
CYCLE; PART II; CERES; BUDGET
AB The Clouds and the Earth's Radiant Energy Systems (CERES) project utilizes radiometric measurements taken aboard the Terra and Aqua spacecrafts to derive the world-class data products needed for climate research. Achieving the exceptional fidelity of the CERES data products, however, requires a considerable amount of processing to assure quality and to verify accuracy and precision, which results in the CERES data being released more than 6 months after the satellite observations. For most climate studies such delays are of little consequence; however, there are a significant number of near-real time uses for CERES data products. The Fast Longwave and Shortwave Radiative Flux (FLASHFlux) data product was therefore developed to provide a rapid release version of the CERES results, which could be made available to the research and applications communities within 1 week of the satellite observations by exchanging some accuracy for speed. FLASHFlux has both achieved this 1-week processing objective and demonstrated the ability to provide remarkably good agreement when compared with the CERES data products for both the instantaneous single-scanner footprint (SSF) fluxes and the time-and space-averaged (TISA) fluxes. This paper describes the methods used to expedite the production of the FLASHFlux SSF fluxes by utilizing data from the CERES and Moderate Resolution Imaging Spectroradiometer instruments, as well as other meteorological sources. This paper also reports on the validation of the FLASHFlux SSF results against ground-truth measurements and the intercomparison of FLASHFlux and CERES SSF results. A complementary paper will discuss the production and validation of the FLASHFlux TISA fluxes.
C1 [Kratz, David P.; Stackhouse, Paul W., Jr.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
[Gupta, Shashi K.; Wilber, Anne C.; Sawaengphokhai, Parnchai] Sci Syst & Applicat Inc, Hampton, VA USA.
[McGarragh, Greg R.] Colorado State Univ, Ft Collins, CO 80523 USA.
RP Kratz, DP (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM david.p.kratz@nasa.gov
FU NASA Science Mission Directorate as part of the CERES project
FX ARM data have been made available through the U.S. Department of Energy
as part of the Atmospheric Radiation Measurement Program. GMD data have
been made available through NOAA's Earth System Research
Laboratory/Global Monitoring Division-Radiation (G-RAD). SURFRAD data
have been made available through NOAA's Air Resources Laboratory/Surface
Radiation Research Branch. Snow and ice data were provided through the
National Snow and Ice Data Center. The authors thank D. A. Rutan for
providing access to the CERES/ARM Validation Experiment (CAVE) database,
and A. C. Edwards and J. C. Mikovitz for providing programming
assistance. The authors would also like to thank G. G. Gibson and N. G.
Loeb for providing valuable advice and suggestions regarding the
manuscript. This research was supported through the NASA Science Mission
Directorate as part of the CERES project.
NR 59
TC 4
Z9 4
U1 0
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD APR
PY 2014
VL 53
IS 4
BP 1059
EP 1079
DI 10.1175/JAMC-D-13-061.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AH9GG
UT WOS:000336449300017
ER
PT J
AU Kulie, MS
Hiley, MJ
Bennartz, R
Kneifel, S
Tanelli, S
AF Kulie, Mark S.
Hiley, Michael J.
Bennartz, Ralf
Kneifel, Stefan
Tanelli, Simone
TI Triple-Frequency Radar Reflectivity Signatures of Snow: Observations and
Comparisons with Theoretical Ice Particle Scattering Models
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID SIZE SPECTRA; CLOUD ICE; MICROWAVE-FREQUENCIES; PRECIPITATION RADAR;
WAKASA BAY; DISTRIBUTIONS; PARAMETERIZATION; APPROXIMATION; MIDLATITUDE;
SNOWFLAKES
AB An observation-based study is presented that utilizes aircraft data from the 2003 Wakasa Bay Advanced Microwave Scanning Radiometer Precipitation Validation Campaign to assess recent advances in the modeling of microwave scattering properties of nonspherical ice particles in the atmosphere. Previous work has suggested that a triple-frequency (Ku-Ka-W band) reflectivity framework appears capable of identifying key microphysical properties of snow, potentially providing much-needed constraints on significant sources of uncertainty in current snowfall retrieval algorithms used for microwave remote sensing instruments. However, these results were based solely on a modeling framework. In contrast, this study considers the triple-frequency approach from an observational perspective using airborne radar observations from the Wakasa Bay field campaign. After accounting for several challenges with the observational dataset, such as beam mismatching and attenuation, observed dual-wavelength ratio results are presented that confirm both the utility of a multifrequency approach to snowfall retrieval and the validity of the unique signatures predicted by complex aggregate ice particle scattering models. This analysis provides valuable insight into the microphysics of frozen precipitation that can in turn be applied to more readily available single-and dual-frequency systems, providing guidance for future precipitation retrieval algorithms.
C1 [Kulie, Mark S.; Hiley, Michael J.; Bennartz, Ralf] Univ Madison, Space Sci & Engn Ctr, Dept Atmospher & Ocean Sci, Madison, WI 53706 USA.
[Kneifel, Stefan] Univ Cologne, Inst Geophys & Meteorol, Cologne, Germany.
[Tanelli, Simone] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Kulie, MS (reprint author), Univ Madison, Space Sci & Engn Ctr, 1225 W Dayton St, Madison, WI 53706 USA.
EM mskulie@wisc.edu
RI Kneifel, Stefan/A-2044-2015; Kulie, Mark/C-3289-2011
OI Kneifel, Stefan/0000-0003-2220-2968; Kulie, Mark/0000-0003-1400-1007
FU NASA [NNX10AG83G, NNX12AQ76G, NNX13AG47G]; Precipitation Measurement
Mission Program; Aerosol Clouds and Ecosystems Science Working Group
FX This work was partially supported by NASA Grants NNX10AG83G, NNX12AQ76G,
and NNX13AG47G. A portion of this research (Tanelli) was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration.
Support by the Precipitation Measurement Mission Program and the Aerosol
Clouds and Ecosystems Science Working Group are acknowledged. Data for
the ACR during the Wakasa Bay Experiment were acquired and processed by
Dr. Richard Austin. The APR-2 deployment was made possible by Dr.
Eastwood Im and Dr. Stephen L. Durden. Constructive comments by three
anonymous reviewers are also gratefully recognized.
NR 55
TC 10
Z9 10
U1 1
U2 17
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD APR
PY 2014
VL 53
IS 4
BP 1080
EP 1098
DI 10.1175/JAMC-D-13-066.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AH9GG
UT WOS:000336449300018
ER
PT J
AU Neigh, CSR
Bolton, DK
Diabate, M
Williams, JJ
Carvalhais, N
AF Neigh, Christopher S. R.
Bolton, Douglas K.
Diabate, Mouhamad
Williams, Jennifer J.
Carvalhais, Nuno
TI An Automated Approach to Map the History of Forest Disturbance from
Insect Mortality and Harvest with Landsat Time-Series Data
SO REMOTE SENSING
LA English
DT Article
DE Landsat; AVHRR; forest; disturbance; mortality; insect; harvest; US;
classification; decision tree
ID MOUNTAIN PINE-BEETLE; REMOTELY SENSED DATA; ACCURACY ASSESSMENT;
UNITED-STATES; BURN SEVERITY; PHOTOSYNTHETIC TRENDS; BUDWORM
DEFOLIATION; LANDSCAPE PATTERNS; SAMPLING DESIGNS; FIRE DISTURBANCE
AB Forests contain a majority of the aboveground carbon (C) found in ecosystems, and understanding biomass lost from disturbance is essential to improve our C-cycle knowledge. Our study region in the Wisconsin and Minnesota Laurentian Forest had a strong decline in Normalized Difference Vegetation Index (NDVI) from 1982 to 2007, observed with the National Ocean and Atmospheric Administration's (NOAA) series of Advanced Very High Resolution Radiometer (AVHRR). To understand the potential role of disturbances in the terrestrial C-cycle, we developed an algorithm to map forest disturbances from either harvest or insect outbreak for Landsat time-series stacks. We merged two image analysis approaches into one algorithm to monitor forest change that included: (1) multiple disturbance index thresholds to capture clear-cut harvest; and (2) a spectral trajectory-based image analysis with multiple confidence interval thresholds to map insect outbreak. We produced 20 maps and evaluated classification accuracy with air-photos and insect air-survey data to understand the performance of our algorithm. We achieved overall accuracies ranging from 65% to 75%, with an average accuracy of 72%. The producer's and user's accuracy ranged from a maximum of 32% to 70% for insect disturbance, 60% to 76% for insect mortality and 82% to 88% for harvested forest, which was the dominant disturbance agent. Forest disturbances accounted for 22% of total forested area (7349 km(2)). Our algorithm provides a basic approach to map disturbance history where large impacts to forest stands have occurred and highlights the limited spectral sensitivity of Landsat time-series to outbreaks of defoliating insects. We found that only harvest and insect mortality events can be mapped with adequate accuracy with a non-annual Landsat time-series. This limited our land cover understanding of NDVI decline drivers. We demonstrate that to capture more subtle disturbances with spectral trajectories, future observations must be temporally dense to distinguish between type and frequency in heterogeneous landscapes.
C1 [Neigh, Christopher S. R.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Bolton, Douglas K.] Univ British Columbia, Dept Forest Resources Management, Vancouver, BC V6T 1Z4, Canada.
[Diabate, Mouhamad] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Williams, Jennifer J.] Royal Bot Gardens, Herbarium, Richmond TW9 3AE, Surrey, England.
[Carvalhais, Nuno] Max Planck Inst Biogeochem, D-07701 Jena, Germany.
[Carvalhais, Nuno] Univ Nova Lisboa, FCT, DCEA, P-2829516 Caparica, Portugal.
RP Bolton, DK (reprint author), Univ British Columbia, Dept Forest Resources Management, Vancouver, BC V6T 1Z4, Canada.
EM christopher.s.neigh@nasa.gov; doug.k.bolton@alumni.ubc.ca;
mdiabate@gmail.com; jenjwilliams@gmail.com; ncarval@bgc-jena.mpg.de
RI Neigh, Christopher/D-4700-2012;
OI Neigh, Christopher/0000-0002-5322-6340; Carvalhais,
Nuno/0000-0003-0465-1436
FU NASA's Terrestrial Ecology program [NNH08ZDA001N-TE,
NNH10ZDA001N-CARBON]
FX This study was made possible by NASA's Terrestrial Ecology program under
grants NNH08ZDA001N-TE and NNH10ZDA001N-CARBON.
NR 91
TC 8
Z9 8
U1 1
U2 26
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD APR
PY 2014
VL 6
IS 4
BP 2782
EP 2808
DI 10.3390/rs6042782
PG 27
WC Remote Sensing
SC Remote Sensing
GA AI3FT
UT WOS:000336746900010
ER
PT J
AU Bhatt, R
Doelling, DR
Wu, AS
Xiong, XX
Scarino, BR
Haney, CO
Gopalan, A
AF Bhatt, Rajendra
Doelling, David R.
Wu, Aisheng
Xiong, Xiaoxiong (Jack)
Scarino, Benjamin R.
Haney, Conor O.
Gopalan, Arun
TI Initial Stability Assessment of S-NPP VIIRS Reflective Solar Band
Calibration Using Invariant Desert and Deep Convective Cloud Targets
SO REMOTE SENSING
LA English
DT Article
DE satellite calibration; S-NPP VIIRS; radiometric stability; MODIS; CERES;
invariant calibration targets
ID ANGULAR-DISTRIBUTION MODELS; RADIATIVE FLUX ESTIMATION; ENERGY SYSTEM
INSTRUMENT; NEAR-INFRARED CHANNELS; TERRA SATELLITE; ATMOSPHERE; SITES;
VALIDATION; SENSORS; AVHRR
AB The latest CERES FM-5 instrument launched onboard the S-NPP spacecraft will use the VIIRS visible radiances from the NASA Land Product Evaluation and Analysis Tool Elements (PEATE) product for retrieving the cloud properties associated with its TOA flux measurement. In order for CERES to provide climate quality TOA flux datasets, the retrieved cloud properties must be consistent throughout the record, which is dependent on the calibration stability of the VIIRS imager. This paper assesses the NASA calibration stability of the VIIRS reflective solar bands using the Libya-4 desert and deep convective clouds (DCC). The invariant targets are first evaluated for temporal natural variability. It is found for visible (VIS) bands that DCC targets have half of the variability of Libya-4. For the shortwave infrared (SWIR) bands, the desert has less variability. The brief VIIRS record and target variability inhibits high confidence in identifying any trends that are less than +/- 0.6%/yr for most VIS bands, and +/- 2.5%/yr for SWIR bands. None of the observed invariant target reflective solar band trends exceeded these trend thresholds. Initial assessment results show that the VIIRS data have been consistently calibrated and that the VIIRS instrument stability is similar to or better than the MODIS instrument.
C1 [Bhatt, Rajendra; Scarino, Benjamin R.; Haney, Conor O.; Gopalan, Arun] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Doelling, David R.] NASA, Langley Res Ctr, Hampton, VA 23666 USA.
[Wu, Aisheng] Sigma Space Corp, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong (Jack)] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Bhatt, R (reprint author), Sci Syst & Applicat Inc, 1 Enterprise Pkwy, Hampton, VA 23666 USA.
EM rajendra.bhatt@nasa.gov; david.r.doelling@nasa.gov;
Aisheng.Wu@sigmaspace.com; Xiaoxiong.Xiong.1@gsfc.nasa.gov;
benjamin.r.scarino@nasa.gov; conor.o.haney@nasa.gov;
arun.gopalan-1@nasa.gov
RI Richards, Amber/K-8203-2015
FU National Aeronautics and Space Administration Earth Science Enterprise
Office through the CERES Program; National Aeronautics and Space
Administration Earth Science Enterprise Office through CLARREO Program;
National Aeronautics and Space Administration Earth Science Enterprise
Office through Satellite Calibration Interconsistency Program; National
Atmospheric and Oceanic Administration Climate Data Records Program [MOA
IA1-1016]
FX This work was supported by the National Aeronautics and Space
Administration Earth Science Enterprise Office through the CERES,
CLARREO and the Satellite Calibration Interconsistency Programs and by
the National Atmospheric and Oceanic Administration Climate Data Records
Program through Grant MOA IA1-1016.
NR 32
TC 21
Z9 21
U1 0
U2 5
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD APR
PY 2014
VL 6
IS 4
BP 2809
EP 2826
DI 10.3390/rs6042809
PG 18
WC Remote Sensing
SC Remote Sensing
GA AI3FT
UT WOS:000336746900011
ER
PT J
AU Anyamba, A
Small, JL
Tucker, CJ
Pak, EW
AF Anyamba, Assaf
Small, Jennifer L.
Tucker, Compton J.
Pak, Edwin W.
TI Thirty-two Years of Sahelian Zone Growing Season Non-Stationary NDVI3g
Patterns and Trends
SO REMOTE SENSING
LA English
DT Article
DE Sahel; NDVI; rainfall; climate record; growing season; standardized
anomalies; extremes; trend patterns
ID DIFFERENCE VEGETATION INDEX; AFRICAN SAHEL; SPECTRAL REFLECTANCE; SAHARA
DESERT; SOIL-EROSION; WEST-AFRICA; NOAA-AVHRR; EL-NINO; RAINFALL;
CLIMATE
AB We update the Global Inventory Modeling and Mapping Studies (GIMMS) analysis of Sahelian vegetation dynamics and trends using the normalized difference vegetation index (NDVI; version 3g) 1981 to 2012 data set. We compare the annual NDIV3g and July to October growing season averages with the three rainfall data sets: the Africa Rainfall Climatology from 1983 to 2012, the Variability Analyses of Surface Climate Observations Version-1.1 from 1951 to 2000, and the Nicholson ground-station precipitation rainfall data from 1981 to 1994. We use the Nicholson ground-station annual precipitation data to determine the reliability of the two continental precipitation data sets for specific locations and specific times, extrapolate these confirmed relationships over the Sahelian Zone from 1983 to 2012 with the Africa Rainfall Climatology, and then place these zonal findings within the 1951 to 2000 record of the Variability Analyses of Surface Climate Observations Version-1.1 precipitation data set. We confirm the extreme nature of the 1984-1985 Sahelian drought, a signature event that marked the minima during the 1980s desiccation period followed within ten years by near-maxima rainfall event in 1994 and positive departures is NDVI, marking beginning of predominantly wetter conditions that have persisted to 2012. We also show the NDVI3g data capture effective rainfall, the rainfall that is utilized by plants to grow, as compared to rainfall that evaporates or is runoff. Using our effective rainfall concept, we estimate average effective rainfall for the entire Sahelian Zone for the 1984 extreme drought was 223 mm/yr as compared to 406 mm/yr in during the 1994 wet period. We conclude that NDVI3g data can used as a proxy for analyzing and interpreting decadal-scale land surface variability and trends over semi arid-lands.
C1 [Anyamba, Assaf; Small, Jennifer L.; Tucker, Compton J.; Pak, Edwin W.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, GIMMS Grp, Greenbelt, MD 20771 USA.
RP Anyamba, A (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, GIMMS Grp, Code 618-0, Greenbelt, MD 20771 USA.
EM assaf.anyamba@nasa.gov; Jennifer.l.small@nasa.gov;
Compton.j.tucker@nasa.gov; edwin.w.pak@nasa.gov
FU USDA Foreign Agricultural Service Global Agricultural Monitoring project
FX This work was made possible by funding from USDA Foreign Agricultural
Service Global Agricultural Monitoring project through its support of
our operational GIMMS NOAA AVHRR NDVI production that is critical input
into the NDVI3g long term series data set. We want to extend thanks to
three anonymous reviewers whose comments and critical reviews served to
improve this manuscript.
NR 64
TC 18
Z9 21
U1 1
U2 28
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD APR
PY 2014
VL 6
IS 4
BP 3101
EP 3122
DI 10.3390/rs6043101
PG 22
WC Remote Sensing
SC Remote Sensing
GA AI3FT
UT WOS:000336746900025
ER
PT J
AU Groce, A
Havelund, K
Holzmann, G
Joshi, R
Xu, RG
AF Groce, Alex
Havelund, Klaus
Holzmann, Gerard
Joshi, Rajeev
Xu, Ru-Gang
TI Establishing flight software reliability: testing, model checking,
constraint-solving, monitoring and learning
SO ANNALS OF MATHEMATICS AND ARTIFICIAL INTELLIGENCE
LA English
DT Article
DE File systems; Testing; Model checking; Verification; Flight software;
Formal proof
ID RULE SYSTEMS; FORMAL VERIFICATION; SYMBOLIC EXECUTION; TEST-GENERATION;
COMPILER; PROGRAMS; SOLVER; EAGLE; TOOL
AB In this paper we discuss the application of a range of techniques to the verification of mission-critical flight software at NASA's Jet Propulsion Laboratory. For this type of application we want to achieve a higher level of confidence than can be achieved through standard software testing. Unfortunately, given the current state of the art, especially when efforts are constrained by the tight deadlines and resource limitations of a flight project, it is not feasible to produce a rigorous formal proof of correctness of even a well-specified stand-alone module such as a file system (much less more tightly coupled or difficult-to-specify modules). This means that we must look for a practical alternative in the area between traditional testing and proof, as we attempt to optimize rigor and coverage. The approaches we describe here are based on testing, model checking, constraint-solving, monitoring, and finite-state machine learning, in addition to static code analysis. The results we have obtained in the domain of file systems are encouraging, and suggest that for more complex properties of programs with complex data structures, it is possibly more beneficial to use constraint solvers to guide and analyze execution (i.e., as in testing, even if performed by a model checking tool) than to translate the program and property into a set of constraints, as in abstraction-based and bounded model checkers. Our experience with non-file-system flight software modules shows that methods even further removed from traditional static formal methods can be assisted by formal approaches, yet readily adopted by test engineers and software developers, even as the key problem shifts from test generation and selection to test evaluation.
C1 [Groce, Alex] Oregon State Univ, Sch Elect Engn & Comp Sci, Corvallis, OR 97331 USA.
[Havelund, Klaus; Holzmann, Gerard; Joshi, Rajeev] CALTECH, Jet Prop Lab, Lab Reliable Software, Pasadena, CA 91109 USA.
[Xu, Ru-Gang] Univ Calif Los Angeles, Dept Comp Sci, Los Angeles, CA 90095 USA.
RP Groce, A (reprint author), Oregon State Univ, Sch Elect Engn & Comp Sci, Corvallis, OR 97331 USA.
EM agroce@gmail.com
FU National Aeronautics and Space Administration; NASA ESAS 6G
FX The research described in this publication was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. Funding
was also provided by NASA ESAS 6G. (C) 2008. All Rights Reserved
NR 102
TC 3
Z9 3
U1 2
U2 13
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1012-2443
EI 1573-7470
J9 ANN MATH ARTIF INTEL
JI Ann. Math. Artif. Intell.
PD APR
PY 2014
VL 70
IS 4
SI SI
BP 315
EP 349
DI 10.1007/s10472-014-9408-8
PG 35
WC Computer Science, Artificial Intelligence; Mathematics, Applied
SC Computer Science; Mathematics
GA AH8DZ
UT WOS:000336365800002
ER
PT J
AU Stecker, FW
AF Stecker, Floyd W.
TI Limiting superluminal electron and neutrino velocities using the 2010
Crab Nebula flare and the IceCube PeV neutrino events
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Lorentz invariance; Neutrino; Electron
ID HIGH-ENERGY NEUTRINOS; SN1987A; TESTS; BURST
AB The observation of two PeV-scale neutrino events reported by Ice Cube allows one to place constraints on Lorentz invariance violation (LIV) in the neutrino sector. After first arguing that at least one of the PeV IceCube events was of extragalactic origin, I derive an upper limit for the difference between putative superluminal neutrino and electron velocities of <=similar to 5.6 x 10(-19) in units where c = 1, confirming that the observed PeV neutrinos could have reached Earth from extragalactic sources. I further derive a new constraint on the superluminal electron velocity, obtained from the observation of synchrotron radiation from the Crab Nebula flare of September, 2010. The inference that the >1 GeV gamma-rays from synchrotron emission in the flare were produced by electrons of energy up to similar to 5.1 PeV indicates the non-occurrence of vacuum Cerenkov radiation by these electrons. This implies a new, strong constraint on superluminal electron velocities delta(e) <=similar to 5 x 10(-21). It immediately follows that one then obtains an upper limit on the superluminal neutrino velocity alone of delta(v) <= similar to 5.6 x 10(-19), many orders of magnitude better than the time-of-flight constraint from the SN1987A neutrino burst. However, if the electrons are sublurninal the constraint on |delta(e)| <=similar to 8 x 10(-17), obtained from the Crab Nebula gamma-ray spectrum, places a weaker constraint on superluminal neutrino velocity of delta(v) <=similar to 8 x 10(-17). Published by Elsevier B.V.
C1 NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Stecker, FW (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
EM floyd.w.stecker@nasa.gov
NR 41
TC 10
Z9 10
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
EI 1873-2852
J9 ASTROPART PHYS
JI Astropart Phys.
PD APR
PY 2014
VL 56
BP 16
EP 18
DI 10.1016/j.astropartphys.2014.02.007
PG 3
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AH7UO
UT WOS:000336341000003
ER
PT J
AU Palucis, MC
Dietrich, WE
Hayes, AG
Williams, RME
Gupta, S
Mangold, N
Newsom, H
Hardgrove, C
Calef, F
Sumner, DY
AF Palucis, Marisa C.
Dietrich, William E.
Hayes, Alexander G.
Williams, Rebecca M. E.
Gupta, Sanjeev
Mangold, Nicholas
Newsom, Horton
Hardgrove, Craig
Calef, Fred, III
Sumner, Dawn Y.
TI The origin and evolution of the Peace Vallis fan system that drains to
the Curiosity landing area, Gale Crater, Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Peace Vallis Fan; MSL; Gale Crater; Mars
ID LARGE ALLUVIAL FANS; SEDIMENTARY-ROCKS; CLIMATE; CONSTRAINTS;
ANTARCTICA; DEPOSITS; RIVERS; MOUND; WATER
AB The landing site for the Curiosity rover is located at the distal end of the Peace Vallis fan in Gale Crater. Peace Vallis fan covers 80km(2) and is fed by a 730km(2) catchment, which drains an upland plains area through a 15km wide gap in the crater rim. Valley incision into accumulated debris delivered sediment through a relatively low density valley network to a main stem channel to the fan. An estimated total fan volume of 0.9km(3) matches the calculated volume of removal due to valley incision (0.8km(3)) and indicates a mean thickness of 9m. The fan profile is weakly concave up with a mean slope of 1.5% for the lower portion. Numerous inverted channels outcrop on the western surface of the fan, but on the eastern portion such channels are rare suggesting a change in process from distributary channel domination on the west to sheet flow on the eastern portion of the fan. Runoff (discharge/watershed area) to produce the fan is estimated to be more than 600m, perhaps as much as 6000m, indicating a hydrologic cycle that likely lasted at least thousands of years. Atmospheric precipitation (possibly snow) not seepage produced the runoff. Based on topographic data, Peace Vallis fan likely onlapped Bradbury Rise and spilled into a topographic low to the east of the rise. This argues that the light-toned fractured terrain within this topographic low corresponds to the distal deposits of Peace Vallis fan, and in such a setting, lacustrine deposits are expected.
C1 [Palucis, Marisa C.; Dietrich, William E.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Hayes, Alexander G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Williams, Rebecca M. E.] Planetary Sci Inst, Tucson, AZ USA.
[Gupta, Sanjeev] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London, England.
[Mangold, Nicholas] Univ Nantes, Lab Planetol & Geodynam Nantes, CNRS UMR 6112, Nantes, France.
[Newsom, Horton] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
[Hardgrove, Craig] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Calef, Fred, III] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA.
[Sumner, Dawn Y.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA.
RP Palucis, MC (reprint author), Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
EM mpalucis@berkeley.edu
RI Hayes, Alexander/P-2024-2014
OI Hayes, Alexander/0000-0001-6397-2630
FU NASA under the Mars Program Office
FX This research was conducted for the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA under the
Mars Program Office. We would like to thank Alan Howard, the entire MSL
team, but especially John Grotzinger, Bernard Hallet, Ron Sletten, and
Mike Malin for insightful discussions along the way. We greatly
appreciate the comments and suggestions provided by our reviewers,
especially those from Bob Craddock. We also thank the teams responsible
for the orbital data, namely, the HiRISE, CTX, and HRSC teams. We give
special thanks to Malin Space Science Systems, the USGS at Flagstaff,
and Scott Mansfield, Jonathan Joseph, and Thomas Gautier from Cornell
for image and data processing.
NR 58
TC 28
Z9 28
U1 3
U2 27
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR
PY 2014
VL 119
IS 4
BP 705
EP 728
DI 10.1002/2013JE004583
PG 24
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AH6BF
UT WOS:000336215000001
ER
PT J
AU Hamilton, VE
Vasavada, AR
Sebastian, E
Juarez, MD
Ramos, M
Armiens, C
Arvidson, RE
Carrasco, I
Christensen, PR
De Pablo, MA
Goetz, W
Gomez-Elvira, J
Lemmon, MT
Madsen, MB
Martin-Torres, FJ
Martinez-Frias, J
Molina, A
Palucis, MC
Rafkin, SCR
Richardson, MI
Yingst, RA
Zorzano, MP
AF Hamilton, Victoria E.
Vasavada, Ashwin R.
Sebastian, Eduardo
Juarez, Manuel de la Torre
Ramos, Miguel
Armiens, Carlos
Arvidson, Raymond E.
Carrasco, Isaias
Christensen, Philip R.
De Pablo, Miguel A.
Goetz, Walter
Gomez-Elvira, Javier
Lemmon, Mark T.
Madsen, Morten B.
Javier Martin-Torres, F.
Martinez-Frias, Jesus
Molina, Antonio
Palucis, Marisa C.
Rafkin, Scot C. R.
Richardson, Mark I.
Yingst, R. Aileen
Zorzano, Maria-Paz
TI Observations and preliminary science results from the first 100 sols of
MSL Rover Environmental Monitoring Station ground temperature sensor
measurements at Gale Crater
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars; ground temperature; thermal inertia; thermophysics
ID THERMAL EMISSION SPECTROMETER; CANDIDATE LANDING SITES; IMAGING-SYSTEM
THEMIS; SURFACE-PROPERTIES; OPTICAL DEPTH; MARS; INERTIA; WATER;
MISSION; ICE
AB We describe preliminary results from the first 100 sols of ground temperature measurements along the Mars Science Laboratory's traverse from Bradbury Landing to Rocknest in Gale. The ground temperature data show long-term increases in mean temperature that are consistent with seasonal evolution. Deviations from expected temperature trends within the diurnal cycle are observed and may be attributed to rover and environmental effects. Fits to measured diurnal temperature amplitudes using a thermal model suggest that the observed surfaces have thermal inertias in the range of 265-375J m(-2) K-1 s(-1/2), which are within the range of values determined from orbital measurements and are consistent with the inertias predicted from the observed particle sizes on the uppermost surface near the rover. Ground temperatures at Gale Crater appear to warm earlier and cool later than predicted by the model, suggesting that there are multiple unaccounted for physical conditions or processes in our models. Where the Mars Science Laboratory (MSL) descent engines removed a mobile layer of dust and fine sediments from over rockier material, the diurnal temperature profile is closer to that expected for a homogeneous surface, suggesting that the mobile materials on the uppermost surface may be partially responsible for the mismatch between observed temperatures and those predicted for materials having a single thermal inertia. Models of local stratigraphy also implicate thermophysical heterogeneity at the uppermost surface as a potential contributor to the observed diurnal temperature cycle.
Key Points Diurnal ground temperatures vary with location Diurnal temperature curves are not well matched by a homogeneous thermal model GTS data are consistent with a varied stratigraphy and thermophysical properties
C1 [Hamilton, Victoria E.; Rafkin, Scot C. R.] Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Vasavada, Ashwin R.; Juarez, Manuel de la Torre] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Sebastian, Eduardo; Armiens, Carlos; Carrasco, Isaias; Gomez-Elvira, Javier; Javier Martin-Torres, F.; Martinez-Frias, Jesus; Molina, Antonio; Zorzano, Maria-Paz] Ctr Astrobiol CSIC INTA, Madrid, Spain.
[Ramos, Miguel; Molina, Antonio] Univ Alcala De Henares, Dept Fis & Matemat, Alcala De Henares, Spain.
[Arvidson, Raymond E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Christensen, Philip R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[De Pablo, Miguel A.] Univ Alcala De Henares, Dept Geol Geog & Medio Ambiente, Alcala De Henares, Spain.
[Goetz, Walter] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Lemmon, Mark T.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA.
[Madsen, Morten B.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Javier Martin-Torres, F.] Inst Andaluz Ciencias Tierra CSIC UGR, Granada, Spain.
[Martinez-Frias, Jesus] Inst Geociencias CSIC UCM, Madrid, Spain.
[Palucis, Marisa C.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Richardson, Mark I.] Ashima Res, Pasadena, CA USA.
[Yingst, R. Aileen] Planetary Sci Inst, Tucson, AZ USA.
RP Hamilton, VE (reprint author), Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
EM hamilton@boulder.swri.edu
RI de Pablo, Miguel Angel/J-6442-2014; Gomez-Elvira, Javier/K-5829-2014;
Ramos, Miguel/K-2230-2014; Lemmon, Mark/E-9983-2010; Zorzano,
Maria-Paz/C-5784-2015; Martin-Torres, Francisco Javier/G-6329-2015;
Zorzano, Maria-Paz/F-2184-2015
OI Molina, Antonio/0000-0002-5038-2022; de Pablo, Miguel
Angel/0000-0002-4496-2741; Gomez-Elvira, Javier/0000-0002-9068-9846;
Ramos, Miguel/0000-0003-3648-6818; Lemmon, Mark/0000-0002-4504-5136;
Zorzano, Maria-Paz/0000-0002-4492-9650; Martin-Torres, Francisco
Javier/0000-0001-6479-2236; Zorzano, Maria-Paz/0000-0002-4492-9650
FU Mars Science Laboratory; Mars Odyssey Participating Scientist Programs;
Economy and Competitivity Ministry [AYA2011-25720, AYA2012-38707]; Mars
Science Laboratory project; Deutsche Forschungsgemeinschaft (DFG) [GO
2288/1-1]; Danish Council for Independent Research/Natural Sciences
(FNU) [0602-02713B]
FX V.E.H. is supported by the Mars Science Laboratory and 2001 Mars Odyssey
Participating Scientist Programs. E. S., C. A., M. R., I. C., J.G.-E.,
M. A. D. P., J.M.-T., and M.-P.Z. are supported by the Economy and
Competitivity Ministry (projects AYA2011-25720 and AYA2012-38707). A.
V., M. T. L., and M.T.J. are supported by the Mars Science Laboratory
project. W. G. acknowledges partial funding by the Deutsche
Forschungsgemeinschaft (DFG grant GO 2288/1-1). M. B. M. is supported by
the Danish Council for Independent Research/Natural Sciences (FNU grant
0602-02713B). We greatly appreciate all of the scientists and engineers
who spent many years working to make the MSL mission such a success. We
also thank the MSL Science Team for their support of the REMS
investigation, and we deeply appreciate the REMS PULs and PDLs (who do
the daily hard work of planning and validating REMS data, usually in the
middle of the Spanish night). We are grateful to Tim Parker and Fred
Calef at JPL for rapid updates to and information about the rover
localization data. Others who have contributed their time and/or advice
include Elena McCartney (MSSS), Larry Edwards (NASA Ames), the MSLICE
team at JPL, Josh Bandfield (SSI), Hugh Kieffer (Celestial Reasonings),
Than Putzig (SwRI), Bob Haberle (NASA Ames), F. Scott Anderson (SwRI),
Chris Edwards (Caltech), Mike Smith (GSFC), Mike Wolff (SSI), Jonathan
Hill (ASU), Kelly Bender (ASU), Dale Noss (ASU), and Kimm Murray (ASU).
Last, but definitely not the least, we thank Josh Bandfield and an
anonymous reviewer for thorough, constructive critiques that helped
improve the manuscript.
NR 81
TC 17
Z9 17
U1 0
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR
PY 2014
VL 119
IS 4
BP 745
EP 770
DI 10.1002/2013JE004520
PG 26
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AH6BF
UT WOS:000336215000003
ER
PT J
AU Stephan, K
Jaumann, R
De Sanctis, MC
Tosi, F
Ammannito, E
Krohn, K
Zambon, F
Marchi, S
Ruesch, O
Matz, KD
Preusker, F
Roatsch, T
Raymond, CA
Russell, CT
AF Stephan, K.
Jaumann, R.
De Sanctis, M. C.
Tosi, F.
Ammannito, E.
Krohn, K.
Zambon, F.
Marchi, S.
Ruesch, O.
Matz, K. -D.
Preusker, F.
Roatsch, T.
Raymond, C. A.
Russell, C. T.
TI Small fresh impact craters on asteroid 4 Vesta: A compositional and
geological fingerprint
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Vesta; asteroid; surface; composition
ID DIFFUSE-REFLECTANCE SPECTRA; DAWN MISSION; HED METEORITES; DARK
MATERIAL; SOLAR-SYSTEM; PARENT BODY; SURFACE; DIOGENITES; MINERALS;
HETEROGENEITY
AB Small morphologically fresh impact craters (<10km in diameter) on Vesta's surface with a photometrically distinct ejecta blanket are expected to represent fresh surface material and thus provide the opportunity to study the composition of the unweathered surface. Dawn-Framing Camera and Visual and Infrared Spectrometer (VIR) data reveal impact craters with bright, dark, and mixed, i.e., partly bright and dark, ejecta existing on Vesta's surface, which not only differ in the visible albedo from their surroundings but also in their composition. Differences in the composition are related to the visible albedo and/or the geographic location of the impact craters. Bright ejecta, only seen in the southern Vestan hemisphere, are dominated by howardite/eucrite-like material as expected for Vesta's upper crust. Dark ejecta associated with dark impact craters are dominated by a strongly absorbing, spectrally neutral compound, supporting an origin from carbon-rich impactors. Few impact craters of intermediate albedo in Vesta's southern hemisphere contain material resembling diogenites, which are expected to exist in the deeper parts of Vesta's interior. The geological settings suggest that the diogenite-like material represents a part of a layer of diogenitic material surrounding the Rheasilvia basin or local concentrations of diogenitic material as part of the ejecta excavated during the latter stage of the Rheasilvia impact event. The spectral differences between eucrite- and diogenite-dominated materials also could be verified due to spin-forbidden absorptions in the visible spectral range, which are known from laboratory spectra of pyroxenes, but, which have been identified in the VIR spectra of Vesta for the first time.
Key Points Fresh impact craters reflect Vesta's unweathered surface composition Vesta's surface varies significantly on a local scale Distribution of materials is related to the formation of Rheasilvia basin
C1 [Stephan, K.; Jaumann, R.; Krohn, K.; Matz, K. -D.; Preusker, F.; Roatsch, T.] DLR, Inst Planetary Res, Berlin, Germany.
[Jaumann, R.] Free Univ Berlin, Inst Geosci, Berlin, Germany.
[De Sanctis, M. C.; Tosi, F.; Ammannito, E.; Zambon, F.] INAF IAPS, Ist Astrofis & Planetol Spaziali, Rome, Italy.
[Marchi, S.] NASA, Lunar Sci Inst, Boulder, CO USA.
[Ruesch, O.] Univ Munster, Inst Planetol, D-48149 Munster, Germany.
[Raymond, C. A.] CALTECH, JPL, Pasadena, CA 91125 USA.
[Russell, C. T.] Univ Calif Los Angeles, Inst Geophys, Los Angeles, CA USA.
RP Stephan, K (reprint author), DLR, Inst Planetary Res, Berlin, Germany.
EM Katrin.Stephan@dlr.de
OI De Sanctis, Maria Cristina/0000-0002-3463-4437; Tosi,
Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592
FU ASI-INAF [I/004/12/0]
FX We thank the Dawn engineering and science team for the development,
cruise, orbital insertion, and operations of the Dawn spacecraft at
Vesta. This work was performed at the DLR Institute of Planetary
Research with support from the VIR visible and infrared mapping
spectrometer team at the INAF Institute for Space Astrophysics and
Planetology (IAPS) in Rome, Italy, JPL in Pasadena, and UCLA in Los
Angeles. The VIR team is founded by ASI-INAF grant I/004/12/0.
NR 92
TC 10
Z9 10
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR
PY 2014
VL 119
IS 4
BP 771
EP 797
DI 10.1002/2013JE004388
PG 27
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AH6BF
UT WOS:000336215000004
ER
PT J
AU Hwang, KJ
Goldstein, ML
Vinas, AF
Schriver, D
Ashour-Abdalla, M
AF Hwang, K. -J.
Goldstein, M. L.
Vinas, A. F.
Schriver, D.
Ashour-Abdalla, M.
TI Wave-particle interactions during a dipolarization front event
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Dipolarization front; wave particle interaction; Electron beams;
Whistler waves; plasma heating
ID AURORAL ELECTRON-BEAM; MAGNETIC RECONNECTION; ACCELERATION; CLUSTER;
PLASMA; MAGNETOSPHERE; PROPAGATION; EVOLUTION; NOISE; SHEET
AB We present Cluster observations of wave-particle interactions during an earthward propagating dipolarization front (DF) and associated fast plasma bulk flows detected at the central current sheet in Earth's magnetotail. During this period, flux tubes behind the DF frequently contain more energetic or hotter ions than did the preexisting flux tubes ahead of the DF. On the other hand, electrons within the DF flux tubes heat less, or are even colder, than were the preexisting populations and are often accompanied by superposed isolated beams. At the same time, electrostatic emissions are strongly enhanced over a wide range of frequencies (up to several times the electron cyclotron frequency) behind the DFs. This low-frequency electrostatic wave power is well correlated with ion energization. From linear theory, we find two wave modes: a high-frequency beam mode and a low-frequency whistler mode that are associated with the electron beam component. We attribute the generation of whistlers to electron beams that persist for a while before undergoing rapid thermalization. The existence of isolated beam components behind DFs detected during the 4 s Cluster spin period indicates that DFs either provide a continuous source of electron beams or facilitate a physical process that maintains the beams against rapid thermalization. Our analysis suggests that the earthward motion of the DF flux tube, via Fermi acceleration as the magnetic field lines behind the DF shorten, can lead to the persistent electron beams that generate whistler mode waves, which in turn can heat ions. This scenario, by which free energy in electron beams generates waves that then heat ions, accounts for the Cluster observations of different energization behaviors between electrons and ions behind DFs.
C1 [Hwang, K. -J.; Goldstein, M. L.; Vinas, A. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hwang, K. -J.] Univ Maryland Baltimore Cty, Goddard Planetary & Heliophys Inst, Baltimore, MD 21228 USA.
[Schriver, D.; Ashour-Abdalla, M.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
RP Hwang, KJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Kyoung-Joo.Hwang@nasa.gov
FU NASA's Magnetospheric Multiscale Mission Interdisciplinary Science
(MMS/IDS) grant; Cluster mission; NASA MMS/IDS grant [NNX08A048G]; NASA
[NNX12AD13G]
FX K.J.H., M. L. G., and A. V. were supported, in part, by NASA's
Magnetospheric Multiscale Mission Interdisciplinary Science (MMS/IDS)
grant to the Goddard Space Flight Center and by the Cluster mission.
Maha Ashour-Abdalla and David Schriver were supported by NASA MMS/IDS
grant NNX08A048G and NASA grant NNX12AD13G.
NR 48
TC 10
Z9 10
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 APR
PY 2014
VL 119
IS 4
BP 2484
EP 2493
DI 10.1002/2013JA019259
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH6CP
UT WOS:000336218600010
ER
PT J
AU Omidi, N
Sibeck, D
Gutynska, O
Trattner, KJ
AF Omidi, N.
Sibeck, D.
Gutynska, O.
Trattner, K. J.
TI Magnetosheath filamentary structures formed by ion acceleration at the
quasi-parallel bow shock
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE magnetosheath; ion acceleration; density structures; temperature
structures; Temperature Structures
ID HOT FLOW ANOMALIES; CYCLOTRON ANISOTROPY INSTABILITIES; MAGNETIC-FIELD
VARIATIONS; GLOBAL HYBRID SIMULATION; UPSTREAM SOLAR-WIND; LOW-FREQUENCY
WAVES; EARTHS MAGNETOSHEATH; ULF WAVES; DENSITY-FLUCTUATIONS;
DIAMAGNETIC CAVITIES
AB Results from 2.5-D electromagnetic hybrid simulations show the formation of field-aligned, filamentary plasma structures in the magnetosheath. They begin at the quasi-parallel bow shock and extend far into the magnetosheath. These structures exhibit anticorrelated, spatial oscillations in plasma density and ion temperature. Closer to the bow shock, magnetic field variations associated with density and temperature oscillations may also be present. Magnetosheath filamentary structures (MFS) form primarily in the quasi-parallel sheath; however, they may extend to the quasi-perpendicular magnetosheath. They occur over a wide range of solar wind Alfvenic Mach numbers and interplanetary magnetic field directions. At lower Mach numbers with lower levels of magnetosheath turbulence, MFS remain highly coherent over large distances. At higher Mach numbers, magnetosheath turbulence decreases the level of coherence. Magnetosheath filamentary structures result from localized ion acceleration at the quasi-parallel bow shock and the injection of energetic ions into the magnetosheath. The localized nature of ion acceleration is tied to the generation of fast magnetosonic waves at and upstream of the quasi-parallel shock. The increased pressure in flux tubes containing the shock accelerated ions results in the depletion of the thermal plasma in these flux tubes and the enhancement of density in flux tubes void of energetic ions. This results in the observed anticorrelation between ion temperature and plasma density.
C1 [Omidi, N.] Solana Sci Inc, Solana Beach, CA 92075 USA.
[Sibeck, D.; Gutynska, O.] NASA GSFC, Greenbelt, MD USA.
[Trattner, K. J.] Univ Colorado, LASP, Boulder, CO 80309 USA.
RP Omidi, N (reprint author), Solana Sci Inc, Solana Beach, CA 92075 USA.
EM omidi@solanasci.com
FU NSF [AGS-1007449, AGS-1103227, 1102572]
FX Work for this project was supported by NSF grants AGS-1007449,
AGS-1103227, and 1102572.
NR 76
TC 7
Z9 7
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 APR
PY 2014
VL 119
IS 4
BP 2593
EP 2604
DI 10.1002/2013JA019587
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH6CP
UT WOS:000336218600017
ER
PT J
AU Hajra, R
Echer, E
Tsurutani, BT
Gonzalez, WD
AF Hajra, Rajkumar
Echer, Ezequiel
Tsurutani, Bruce T.
Gonzalez, Walter D.
TI Solar wind-magnetosphere energy coupling efficiency and partitioning:
HILDCAAs and preceding CIR storms during solar cycle 23
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Solar wind-magnetosphere energy coupling efficiency; Magnetospheric
energy partitioning; HILDCAAs; CIR storms; Joule heating; Ring current
injection
ID COROTATING INTERACTION REGIONS; INTERPLANETARY MAGNETIC-FIELD;
MAGNETOPAUSE BOUNDARY-LAYER; GEOMAGNETIC-ACTIVITY; CORONAL HOLES; ALFVEN
WAVES; DIFFUSION-PROCESSES; EPSILON-PARAMETER; EVENTS; AE
AB A quantitative study on the energetics of the solar wind-magnetosphere-ionosphere system during High-Intensity, Long-Duration, Continuous AE Activity (HILDCAA) events for solar cycle 23 (from 1995 through 2008) is presented. For all HILDCAAs, the average energy transferred to the magnetospheric/ionospheric system was similar to 6.3x1016 J, and the ram kinetic energy of the incident solar wind was similar to 7.1x1018 J. For individual HILDCAA events the coupling efficiency, defined as the ratio of the solar wind energy input to the solar wind kinetic energy, varied between 0.3% and 2.8%, with an average value of similar to 0.9%. The solar wind coupling efficiency for corotating interaction region (CIR)-driven storms prior to the HILDCAA events was found to vary from similar to 1% to 5%, with an average value of similar to 2%. Both of these values are lower than the> 5% coupling efficiency noted for interplanetary coronal mass ejection (and sheath)-driven magnetic storms. During HILDCAAs, similar to 67% of the solar wind energy input went into Joule heating, similar to 22% into auroral precipitation, and similar to 11% into the ring current energy. The CIR-storm Joule heating (similar to 49%) was noticeably less than that during HILDCAAs, while the ring current energies were comparable for the two. Joule dissipation was higher for HILDCAAs that followed CIR-storms (88%) than for isolated HILDCAAs (similar to 60%). Possible physical interpretations for the statistical results obtained in this paper are discussed.
C1 [Hajra, Rajkumar; Echer, Ezequiel; Gonzalez, Walter D.] Inst Nacl Pesquisas Espaciais, Sao Paulo, Brazil.
[Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Hajra, R (reprint author), Inst Nacl Pesquisas Espaciais, Sao Paulo, 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); Brazilian
CNPq agency [301233/2011-0]; NASA
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 to 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.
NR 91
TC 10
Z9 10
U1 1
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2014
VL 119
IS 4
BP 2675
EP 2690
DI 10.1002/2013JA019646
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH6CP
UT WOS:000336218600023
ER
PT J
AU Valek, PW
Goldstein, J
McComas, DJ
Fok, MC
Mitchell, DG
AF Valek, P. W.
Goldstein, J.
McComas, D. J.
Fok, M-C.
Mitchell, D. G.
TI Large magnetic storms as viewed by TWINS: A study of the differences in
the medium energy ENA composition
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE magnetic storms; ENA; oxygen; TWINS; medium energy; composition
ID RING CURRENT; INNER MAGNETOSPHERE; GEOMAGNETIC STORM; HYDROGEN; TIME;
SPECTRA; IMAGES; IONS; CIR; O+
AB During large geomagnetic storms (Dst-100 nT), oxygen can become a significant component of the energetic particles of the inner magnetosphere. Until recently, there were no available global observations of the medium energy (<50keV) oxygen populations. Using observations from the Two Wide-angle Imaging Neutral-atom Spectrometers (TWINS) Energetic Neutral Atom (ENA) imagers we present a study of nine large storms of solar cycle 24 as a function of storm phase. For these storms we observe that the H and O ENA fluxes and their temperatures increase in tandem during the storm's initial phase. However, there is no increase in the O+/H+ ratio in the inner magnetosphere until the storm main phase. Also seen during the main phase is an energy dispersion with higher-energy (32keV) H ENAs seen before the arrival of O ENAs of the same energy. The O ENAs take longer to return to prestorm levels during the recovery phases. This longer recovery time is likely because of the large difference between the storm time and prestorm O populations compared to H (i.e., there is always some prestorm H in the inner magnetosphere, but effectively no O prestorm). These results imply that medium-energy O ENAs evolve over long time scales (hours to days) as opposed to the shorter substorm time scales of the higher-energy (>52keV) O ENAs.
C1 [Valek, P. W.; Goldstein, J.; McComas, D. J.] SwRI, San Antonio, TX 78238 USA.
[Valek, P. W.; Goldstein, J.; McComas, D. J.] UTSA, Dept Phys, San Antonio, TX USA.
[Fok, M-C.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Mitchell, D. G.] JHU, Appl Phys Lab, Laurel, MD USA.
RP Valek, PW (reprint author), SwRI, San Antonio, TX 78238 USA.
EM PValek@swri.edu
OI Valek, Philip/0000-0002-2318-8750
FU NASA TWINS mission in NASA's explorer program
FX This work was funded as part of the NASA TWINS mission in NASA's
explorer program. Real-time Dst and SYM-H data were kindly provided by
the World Data Center for Geomagnetism, Kyoto University, Japan. Solar
wind data are from the ACE spacecraft and shifted in time by OMNI.
NR 41
TC 4
Z9 4
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2014
VL 119
IS 4
BP 2819
EP 2835
DI 10.1002/2014JA019782
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH6CP
UT WOS:000336218600030
ER
PT J
AU Korth, H
Anderson, BJ
Gershman, DJ
Raines, JM
Slavin, JA
Zurbuchen, TH
Solomon, SC
McNutt, RL
AF Korth, Haje
Anderson, Brian J.
Gershman, Daniel J.
Raines, Jim M.
Slavin, James A.
Zurbuchen, Thomas H.
Solomon, Sean C.
McNutt, Ralph L., Jr.
TI Plasma distribution in Mercury's magnetosphere derived from MESSENGER
Magnetometer and Fast Imaging Plasma Spectrometer observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Mercury; MESSENGER; magnetosphere; plasma pressure; plasma distribution;
plasma entry
ID KELVIN-HELMHOLTZ INSTABILITY; SOLAR-WIND; MAGNETOTAIL BOUNDARY; GEOTAIL
OBSERVATIONS; ION COMPOSITION; MAGNETIC-FIELD; MAGNETOPAUSE; SHEET;
MAGNETOSHEATH; INSTRUMENT
AB We assess the statistical spatial distribution of plasma in Mercury's magnetosphere from observations of magnetic pressure deficits and plasma characteristics by the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft. The statistical distributions of proton flux and pressure were derived from 10months of Fast Imaging Plasma Spectrometer (FIPS) observations obtained during the orbital phase of the MESSENGER mission. The Magnetometer-derived pressure distributions compare favorably with those deduced from the FIPS observations at locations where depressions in the magnetic field associated with the presence of enhanced plasma pressures are discernible in the Magnetometer data. The magnitudes of the magnetic pressure deficit and the plasma pressure agree on average, although the two measures of plasma pressure may deviate for individual events by as much as a factor of similar to 3. The FIPS distributions provide better statistics in regions where the plasma is more tenuous and reveal an enhanced plasma population near the magnetopause flanks resulting from direct entry of magnetosheath plasma into the low-latitude boundary layer of the magnetosphere. The plasma observations also exhibit a pronounced north-south asymmetry on the nightside, with markedly lower fluxes at low altitudes in the northern hemisphere than at higher altitudes in the south on the same field line. This asymmetry is consistent with particle loss to the southern hemisphere surface during bounce motion in Mercury's offset dipole magnetic field.
C1 [Korth, Haje; Anderson, Brian J.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Gershman, Daniel J.; Raines, Jim M.; Slavin, James A.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Gershman, Daniel J.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
RP Korth, H (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
EM haje.korth@jhuapl.edu
RI Slavin, James/H-3170-2012; McNutt, Ralph/E-8006-2010
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166
FU NASA [NAS5-97271, NASW-00002]
FX The MESSENGER project is supported by the NASA Discovery Program under
contracts NAS5-97271 to The Johns Hopkins University Applied Physics
Laboratory and NASW-00002 to the Carnegie Institution of Washington.
NR 57
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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 APR
PY 2014
VL 119
IS 4
BP 2917
EP 2932
DI 10.1002/2013JA019567
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH6CP
UT WOS:000336218600035
ER
PT J
AU Dong, JR
Ek, M
Hall, D
Peters-Lidard, C
Cosgrove, B
Miller, J
Riggs, G
Xia, YL
AF Dong, Jiarui
Ek, Mike
Hall, Dorothy
Peters-Lidard, Christa
Cosgrove, Brian
Miller, Jeff
Riggs, George
Xia, Youlong
TI Using Air Temperature to Quantitatively Predict the MODIS Fractional
Snow Cover Retrieval Errors over the Continental United States
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Drought; Snowpack; Snow cover; Surface temperature; Seasonal variability
ID DATA ASSIMILATION SYSTEM; WATER EQUIVALENT; ACCURACY ASSESSMENT; MAPPING
ACCURACY; VALIDATION; PRODUCTS; AREA; SNOTEL; DEPTH; NLDAS
AB Understanding and quantifying satellite-based, remotely sensed snow cover uncertainty are critical for its successful utilization. The Moderate Resolution Imaging Spectroradiometer (MODIS) snow cover errors have been previously recognized to be associated with factors such as cloud contamination, snowpack grain sizes, vegetation cover, and topography; however, the quantitative relationship between the retrieval errors and these factors remains elusive. Joint analysis of the MODIS fractional snow cover (FSC) from Collection 6 (C6) and in situ air temperature and snow water equivalent measurements provides a unique look at the error structure of the MODIS C6 FSC products. Analysis of the MODIS FSC dataset over the period from 2000 to 2005 was undertaken over the continental United States (CONUS) with an extensive observational network. When compared to MODIS Collection 5 (C5) snow cover area, the MODIS C6 FSC product demonstrates a substantial improvement in detecting the presence of snow cover in Nevada [30% increase in probability of detection (POD)], especially in the early and late snow seasons; some improvement over California (10% POD increase); and a relatively small improvement over Colorado (2% POD increase). However, significant spatial and temporal variations in accuracy still exist, and a proxy is required to adequately predict the expected errors in MODIS C6 FSC retrievals. A relationship is demonstrated between the MODIS FSC retrieval errors and temperature over the CONUS domain, captured by a cumulative double exponential distribution function. This relationship is shown to hold for both in situ and modeled daily mean air temperature. Both of them are useful indices in filtering out the misclassification of MODIS snow cover pixels and in quantifying the errors in the MODIS C6 product for various hydrological applications.
C1 [Dong, Jiarui; Ek, Mike; Xia, Youlong] NOAA, NCEP, EMC, College Pk, MD 20740 USA.
[Dong, Jiarui; Xia, Youlong] IM Syst Grp, Rockville, MD USA.
[Hall, Dorothy; Miller, Jeff; Riggs, George] NASA, Cryospher Sci Lab, GSFC, Greenbelt, MD USA.
[Peters-Lidard, Christa] NASA, Hydrol Sci Lab, GSFC, Greenbelt, MD USA.
[Cosgrove, Brian] NOAA, NWS, OHD, Silver Spring, MD USA.
[Miller, Jeff] Wyle Inc, Houston, TX USA.
[Riggs, George] SSAI Inc, Lanham, MD USA.
RP Dong, JR (reprint author), NOAA, NCEP, EMC, 5830 Univ Res Ct, College Pk, MD 20740 USA.
EM jiarui.dong@noaa.gov
RI Peters-Lidard, Christa/E-1429-2012
OI Peters-Lidard, Christa/0000-0003-1255-2876
FU NOAA Climate Program Office (CPO) Modeling, Analysis, Predictions, and
Projections (MAPP) program
FX We thank Kingtse Mo from NOAA/NCEP/CPC for her contributions. This work
was directly funded by the NOAA Climate Program Office (CPO) Modeling,
Analysis, Predictions, and Projections (MAPP) program. The NASA EOS
Project supported the participation of D. Hall, J. Miller, and G. Riggs.
NR 55
TC 2
Z9 2
U1 0
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD APR
PY 2014
VL 15
IS 2
BP 551
EP 562
DI 10.1175/JHM-D-13-060.1
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AE7LN
UT WOS:000334179500002
ER
PT J
AU Tokay, A
Roche, RJ
Bashor, PG
AF Tokay, Ali
Roche, Rigoberto J.
Bashor, Paul G.
TI An Experimental Study of Spatial Variability of Rainfall
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Hydrometeorology; In situ atmospheric observations
ID SMALL-SCALE RAINFALL; VALIDATION; RADAR; PRODUCTS; TMPA; QPE
AB Spatial variability of rainfall was studied through a gauge network on the Delmarva Peninsula. The gauge network consists of 11 dual- or triple-tipping-bucket sites ranging from 1- to 150-km separation distances. The time of the tip (0.254 mm) was recorded to a datalogger, and a continuous dataset was available from all sites for over 5 yr (May 2005-July 2010). A three-parameter exponential function was fitted to the paired correlations and the resultant correlation distance was 8-13 km during summer and 51-85 km during winter. The correlation distances showed pronounced year-to-year variability as being 8-43 km and 13-67 km during spring and autumn, respectively. The airmass convection was the main weather system during summer while nor'easters played an important role during winter. The 30-min integration and two-tip rain/no-rain threshold was selected for the base of this study. The correlation distance increased with longer integration periods and was 17 and 32 km for 30 min and 1 h, respectively.
C1 [Tokay, Ali] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Greenbelt, MD USA.
[Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Roche, Rigoberto J.] Florida Int Univ, Miami, FL 33199 USA.
[Bashor, Paul G.] Comp Sci Corp, Wallops Isl, VA USA.
[Bashor, Paul G.] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
RP Tokay, A (reprint author), NASA, Goddard Space Flight Ctr, Code 612-0, Greenbelt, MD 20771 USA.
EM ali.tokay-1@nasa.gov
FU NASA's Global Precipitation Measurement Mission; NASA Goddard Space
Flight Center; Precipitation Measurement Mission (PMM) [NNX07AF45G,
NNX10AJ12G]
FX The second author was a summer intern under NASA's Water Escapes
program; Fernando Miralles of Florida International University is the
principal investigator. Acknowledgements extend to Robert Meneghini of
the NASA Goddard Space Flight Center and S. Joseph Munchak of the
University of Maryland for their valuable comments. Special thanks to
Joseph Turk, Editor of the Journal of Hydrometeorology, for his guidance
throughout the review process. We are also thankful for the constructive
comments from the anonymous reviewers. This study was funded under
NASA's Global Precipitation Measurement Mission under Arthur Hou,
project scientist, NASA Goddard Space Flight Center, and the
Precipitation Measurement Mission (PMM) NNX07AF45G and NNX10AJ12G under
Ramesh Kakar, program scientist, NASA Headquarters. Acknowledgments
extend to Mathew Schwaller, GPM ground validation manager, NASA Goddard
Space Flight Center, for his continuous support.
NR 17
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Z9 8
U1 1
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD APR
PY 2014
VL 15
IS 2
BP 801
EP 812
DI 10.1175/JHM-D-13-031.1
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AE7LN
UT WOS:000334179500017
ER
PT J
AU Panerai, F
Martin, A
Mansour, NN
Sepka, SA
Lachaud, J
AF Panerai, Francesco
Martin, Alexandre
Mansour, Nagi N.
Sepka, Steven A.
Lachaud, Jean
TI Flow-Tube Oxidation Experiments on the Carbon Preform of a
Phenolic-Impregnated Carbon Ablator
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
ID THERMAL RESPONSE; HIGH-TEMPERATURE; PYROLYSIS-GAS; GRAPHITE; PROGRAM;
IMAGE
AB Oxidation experiments on the carbon preform of a phenolic-impregnated carbon ablator were performed in a flow-tube reactor facility, at temperatures between 700 and 1300K, under dry air gas at pressures between 1.6x103 and 6.0x104Pa. Mass loss, volumetric recession and density changes were measured at different test conditions. An analysis of the diffusion/reaction competition within the porous material, based on the Thiele number, allows identification of low temperature and low-pressure conditions to be dominated by in-depth volume oxidation. Experiments above 1000K were found at transition conditions, where diffusion and reaction occur at similar scales. The microscopic oxidation behavior of the fibers was characterized by scanning electron microscopy and energy dispersive x-ray analysis. The material was found to oxidize at specific sites, forming a pitting pattern distributed over the surface of the fibers. Calcium- and oxygen-rich residues from the oxidation reactions were observed at several locations.
C1 [Panerai, Francesco; Martin, Alexandre] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Panerai, Francesco; Martin, Alexandre] Univ Kentucky, Ctr Computat Sci, Lexington, KY 40506 USA.
[Mansour, Nagi N.] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA.
[Sepka, Steven A.] ERC Inc, Moffett Field, CA 94035 USA.
[Lachaud, Jean] Univ Calif Santa Cruz, Moffett Field, CA 94035 USA.
RP Panerai, F (reprint author), Univ Kentucky, Dept Mech Engn, 261 Ralph G Anderson Building, Lexington, KY 40506 USA.
RI Martin, Alexandre/L-9520-2014;
OI Martin, Alexandre/0000-0003-2216-2468; Lachaud, Jean/0000-0001-7397-1025
FU NASA [NNX10CC53P, NNX10AV39A]; Hypersonic Entry, Descent, and Landing
(EDL) Program
FX Financial support to the first author of this work was provided by the
NASA Small Business Innovation Research Phase-2 Award NNX10CC53P and the
NASA Kentucky Experimental Program to Stimulate Competitive Research
Award NNX10AV39A. Support by the Hypersonic Entry, Descent, and Landing
(EDL) Program for the effort is gratefully acknowledged. We thank the
unwavering encouragements by M. J. Wright from the NASA Ames Research
Center and A. M. Calomino from the NASA Langley Research Center. We are
also thankful to J. Chavez Garcia, J. W. Ridge, and M. Gusman from ERC,
Inc. for support on scanning electron microscopy, assistance at the
flow-tube laboratory, and for the training on samples' encapsulation,
respectively. The comments of F. S. Milos and Y. K. Chen from the NASA
Ames Research Center are greatly appreciated.
NR 38
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Z9 6
U1 0
U2 3
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0887-8722
EI 1533-6808
J9 J THERMOPHYS HEAT TR
JI J. Thermophys. Heat Transf.
PD APR
PY 2014
VL 28
IS 2
BP 181
EP 190
DI 10.2514/1.T4265
PG 10
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA AH6GX
UT WOS:000336229800002
ER
PT J
AU Lachaud, J
Mansour, NN
AF Lachaud, Jean
Mansour, Nagi N.
TI Porous-Material Analysis Toolbox Based on OpenFOAM and Applications
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
ID PHENOLIC RESIN; CARBON/PHENOLIC COMPOSITE; PYROLYSIS; ABLATION; HEAT
AB The Porous-material Analysis Toolbox based on OpenFOAM is a fully portable OpenFOAM library. It is implemented to test innovative multiscale physics-based models for reacting porous materials that undergo recession. Current developments are focused on ablative materials. The ablative material response module implemented in the Porous-material Analysis Toolbox relies on an original high-fidelity ablation model. The governing equations are volume-averaged forms of the conservation equations for gas mass, gas species, solid mass, gas momentum, and total energy. It may also simply be used as a state-of-the-art ablation model when the right model options are chosen. As applications, three physical analyses are presented: 1)volume-averaged study of the oxidation of a carbon-fiber preform under dry air, 2)three-dimensional analysis of the pyrolysis gas flow in a porous ablative material sample facing an arcjet, and 3)comparison of a state-of-the-art and a high-fidelity model for the thermal and chemical response of a carbon/phenolic ablative material.
C1 [Lachaud, Jean] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Mansour, Nagi N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lachaud, J (reprint author), Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
EM jlachaud@ucsc.edu; nagi.n.mansour@nasa.gov
OI Lachaud, Jean/0000-0001-7397-1025
FU NASA's Fundamental Aeronautic Program Hypersonics Nasa Research
Announcement (NRA) [NNX12AG47A]; Space Technology Research Grants
Program
FX This research was originally funded by NASA's Fundamental Aeronautic
Program Hypersonics Nasa Research Announcement (NRA) grant NNX12AG47A.
It is currently supported by the Space Technology Research Grants
Program. The authors would like to thank G. Blanquart (Caltech) for
providing a preliminary reduced mechanism of his combustion database.
NR 21
TC 6
Z9 6
U1 1
U2 5
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0887-8722
EI 1533-6808
J9 J THERMOPHYS HEAT TR
JI J. Thermophys. Heat Transf.
PD APR
PY 2014
VL 28
IS 2
BP 191
EP 202
DI 10.2514/1.T4262
PG 12
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA AH6GX
UT WOS:000336229800003
ER
PT J
AU Welsh, T
Burek-Huntington, K
Savage, K
Rosenthal, B
Dubey, JP
AF Welsh, Trista
Burek-Huntington, Kathy
Savage, Kate
Rosenthal, Benjamin
Dubey, J. P.
TI Sarcocystis canis Associated Hepatitis in a Steller Sea Lion (Eumetopias
jubatus) from Alaska
SO JOURNAL OF WILDLIFE DISEASES
LA English
DT Article
ID TOXOPLASMA-GONDII; NEOSPORA-CANINUM; INFECTIONS; PARASITES; NEURONA
AB Sarcocystis canis infection was associated with hepatitis in a Steller sea lion (Eumetopias jubatus). Intrahepatocellular protozoal schizonts were among areas of necrosis and inflammation. The parasite was genetically identical to S. canis and is the first report in a Steller sea lion, indicating another intermediate host species for S. canis.
C1 [Welsh, Trista] Univ Georgia, Coll Vet Med, Athens, GA 30605 USA.
[Burek-Huntington, Kathy] Alaska Vet Pathol Serv, Eagle River, AK 99577 USA.
[Savage, Kate] Natl Marine Fisheries Serv, Protected Resources Div, Juneau, AK 99802 USA.
[Rosenthal, Benjamin; Dubey, J. P.] ARS, USDA, Beltsville Agr Res Ctr, Anim Parasit Dis Lab,BARC East, Beltsville, MD 20705 USA.
RP Welsh, T (reprint author), Flyinvet, 10174 Airpark Loop, Givens Hotsprings, ID 83641 USA.
EM trista.welsh@gmail.com
OI Rosenthal, Benjamin/0000-0002-0224-3773
NR 10
TC 0
Z9 0
U1 2
U2 12
PU WILDLIFE DISEASE ASSOC, INC
PI LAWRENCE
PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA
SN 0090-3558
EI 1943-3700
J9 J WILDLIFE DIS
JI J. Wildl. Dis.
PD APR
PY 2014
VL 50
IS 2
BP 405
EP 408
DI 10.7589/2013-03-079
PG 4
WC Veterinary Sciences
SC Veterinary Sciences
GA AH6JT
UT WOS:000336237900036
PM 24484486
ER
PT J
AU Carrier, MJ
Ngodock, H
Smith, S
Jacobs, G
Muscarella, P
Ozgokmen, T
Haus, B
Lipphardt, B
AF Carrier, Matthew J.
Ngodock, Hans
Smith, Scott
Jacobs, Gregg
Muscarella, Philip
Ozgokmen, Tamay
Haus, Brian
Lipphardt, Bruce
TI Impact of Assimilating Ocean Velocity Observations Inferred from
Lagrangian Drifter Data Using the NCOM-4DVAR
SO MONTHLY WEATHER REVIEW
LA English
DT Article
DE Inverse methods; Variational analysis; Model initialization; Numerical
analysis; modeling; Ocean models
ID VARIATIONAL ASSIMILATION; MODELING SYSTEM; EQUATION; SURFACE;
IMPLEMENTATION; CIRCULATION; FORMULATION
AB Eulerian velocity fields are derived from 300 drifters released in the Gulf of Mexico by The Consortium for Advanced Research on Transport of Hydrocarbon in the Environment (CARTHE) during the summer 2012 Grand Lagrangian Deployment (GLAD) experiment. These data are directly assimilated into the Navy Coastal Ocean Model (NCOM) four-dimensional variational data assimilation (4DVAR) analysis system in a series of experiments to investigate their impact on the model circulation. The NCOM-4DVAR is a newly developed tool for data analysis, formulated for weak-constraint data assimilation based on the indirect representer method. The assimilation experiments take advantage of this velocity data along with other available data sources from in situ and satellite measurements of surface and subsurface temperature and salinity. Three different experiments are done: (i) A nonassimilative NCOM free run, (ii) an assimilative NCOM run that utilizes temperature and salinity observations, and (iii) an assimilative NCOM run that uses temperature and salinity observations as well as the GLAD velocity observations. The resulting analyses and subsequent forecasts are compared to assimilated and future GLAD velocity and temperature/salinity observations to determine the performance of each experiment and the impact of the GLAD data on the analysis and the forecast. It is shown that the NCOM-4DVAR is able to fit the observations not only in the analysis step, but also in the subsequent forecast. It is also found that the GLAD velocity data greatly improves the characterization of the circulation, with the forecast showing a better fit to future GLAD observations than those experiments without the velocity data included.
C1 [Carrier, Matthew J.; Ngodock, Hans; Smith, Scott; Jacobs, Gregg] Naval Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
[Muscarella, Philip] Amer Soc Engn Educ, Washington, DC USA.
[Ozgokmen, Tamay; Haus, Brian] Univ Miami, Miami, FL USA.
[Lipphardt, Bruce] Univ Delaware, Newark, DE USA.
RP Carrier, MJ (reprint author), Naval Res Lab, Stennis Space Ctr, Bldg 1009,Balch Blvd, Stennis Space Ctr, MS 39529 USA.
EM matthew.carrier@nrlssc.navy.mil
FU BP/The Gulf of Mexico Research Initiative (GoMRI) through the Consortium
for Advanced Research on Transport of Hydrocarbon in the Environment
(CARTHE); Office of Naval Research Program Element [0601153N]
FX The authors would like to acknowledge Emanuel Coelho for his work in
processing the GLAD drifter observations into Eulerian velocity
measurements used in this assimilation study. The authors would like to
thank the anonymous reviewers for their helpful comments during the
revision process. The authors would also like to state that this
research was made possible in part by a grant from BP/The Gulf of Mexico
Research Initiative (GoMRI) through the Consortium for Advanced Research
on Transport of Hydrocarbon in the Environment (CARTHE). This work was
also sponsored by the Office of Naval Research Program Element 0601153N
as part of the projects "A Multiscale Approach to Assessing
Predictability of ASW Environment" and "The Rapid Transition Project
(RTP) for 4Dvar NCOM in RELO and COAMPS5 with merged NCODA/NAVDAS-AR."
NR 35
TC 10
Z9 10
U1 0
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD APR
PY 2014
VL 142
IS 4
BP 1509
EP 1524
DI 10.1175/MWR-D-13-00236.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AD7IC
UT WOS:000333436300008
ER
PT J
AU Noble, E
Druyan, LM
Fulakeza, M
AF Noble, Erik
Druyan, Leonard M.
Fulakeza, Matthew
TI The Sensitivity of WRF Daily Summertime Simulations over West Africa to
Alternative Parameterizations. Part I: African Wave Circulation
SO MONTHLY WEATHER REVIEW
LA English
DT Article
DE Africa; Waves; atmospheric; Vorticity; Model evaluation; performance;
Parameterization; Regional models
ID EASTERLY WAVE; WEATHER RESEARCH; MODEL PERFORMANCE; FORECASTING-MODEL;
DATA ASSIMILATION; REGIONAL MODEL; CLIMATE-CHANGE; CONVECTION; ATLANTIC;
MONSOON
AB The performance of the NCAR Weather Research and Forecasting Model (WRF) as a West African regional-atmospheric model is evaluated. The study tests the sensitivity of WRF-simulated vorticity maxima associated with African easterly waves to 64 combinations of alternative parameterizations in a series of simulations in September. In all, 104 simulations of 12-day duration during 11 consecutive years are examined. The 64 combinations combine WRF parameterizations of cumulus convection, radiation transfer, surface hydrology, and PBL physics. Simulated daily and mean circulation results are validated against NASA's Modern-Era Retrospective Analysis for Research and Applications (MERRA) and NCEP/Department of Energy Global Reanalysis 2. Precipitation is considered in a second part of this two-part paper. A wide range of 700-hPa vorticity validation scores demonstrates the influence of alternative parameterizations. The best WRF performers achieve correlations against reanalysis of 0.40-0.60 and realistic amplitudes of spatiotemporal variability for the 2006 focus year while a parallel-benchmark simulation by the NASA Regional Model-3 (RM3) achieves higher correlations, but less realistic spatiotemporal variability. The largest favorable impact on WRF-vorticity validation is achieved by selecting the Grell-Devenyi cumulus convection scheme, resulting in higher correlations against reanalysis than simulations using the Kain-Fritch convection. Other parameterizations have less-obvious impact, although WRF configurations incorporating one surface model and PBL scheme consistently performed poorly. A comparison of reanalysis circulation against two NASA radiosonde stations confirms that both reanalyses represent observations well enough to validate the WRF results. Validation statistics for optimized WRF configurations simulating the parallel period during 10 additional years are less favorable than for 2006.
C1 [Noble, Erik] Univ Colorado, Environm Studies Program, Boulder, CO 80309 USA.
[Noble, Erik] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Druyan, Leonard M.; Fulakeza, Matthew] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
RP Noble, E (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM erik.noble@nasa.gov
FU NASA Cooperative Agreement [NNX11AR61G, NNX11AR63A]; National Science
Foundation [AGS-1000874]
FX The authors gratefully acknowledge the inspiration and encouragement for
this project of the late Professor Thomas T. Warner. We also gratefully
acknowledge many very constructive suggestions of two anonymous
reviewers. EUN was supported by NASA Cooperative Agreement NNX11AR61G.
LMD and MF were supported by National Science Foundation Grant
AGS-1000874 and NASA Cooperative Agreement NNX11AR63A. MERRA data were
obtained from NASA's GMAO website (http://gmao.gsfc.nasa.gov/merra),
NAMMA radiosonde data were obtained from NASA's Global Hydrology Center
website (http://airbornescience.nsstc.nasa.gov/namma), and NCEP
Reanalysis-2 data were provided by the NOAA/ESRL/Physical Sciences
Division, Boulder, Colorado, from their website
(http://www.esrl.noaa.gov/psd).
NR 58
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Z9 4
U1 0
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD APR
PY 2014
VL 142
IS 4
BP 1588
EP 1608
DI 10.1175/MWR-D-13-00194.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AD7IC
UT WOS:000333436300013
ER
PT J
AU Balakrishnan, K
AF Balakrishnan, Kaushik
TI Explosion-driven Rayleigh-Taylor instability in gas-particle mixtures
SO PHYSICS OF FLUIDS
LA English
DT Article
ID RICHTMYER-MESHKOV INSTABILITIES; BUOYANCY-DRAG MODEL; BLAST-WAVE;
NUMERICAL-SIMULATION; HEAT-TRANSFER; SHOCK-TUBE; DISPERSION; BUBBLE;
CLOUDS; SPHERE
AB The structure and growth of an explosion-driven Rayleigh-Taylor instability in gas-particle mixtures is investigated using two-dimensional numerical simulations. Particle concentration and diameter are varied and the growth of the ensuing mixing layer and its dependence on these parameters is investigated. The hydrodynamic structures are subdued and lose their coherence with increase in solid particle concentrations. When the solid particle concentration is fixed but particle diameter varied, a non-monotic behavior is observed. It is found that an intermediate particle size results in the widest mixing zone and degree of mixing. This is due to the differences in the spatial accumulation of the particles as they disperse. Small particles accumulate in the bubbles and around the spikes of the Rayleigh-Taylor structures; intermediate-sized particles in the tips of the spikes and as roots into the driver fluid; large particles accumulate primarily in the spikes and as thin, elongated roots into the driver fluid. Such differences are attributed to the response time or Stokes number of the particles. Finally, future directions for extending the current research are summarized. (C) 2014 AIP Publishing LLC.
C1 [Balakrishnan, Kaushik] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Res Div, Berkeley, CA 94720 USA.
RP Balakrishnan, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kaushikb258@gmail.com
NR 33
TC 3
Z9 3
U1 2
U2 14
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-6631
EI 1089-7666
J9 PHYS FLUIDS
JI Phys. Fluids
PD APR
PY 2014
VL 26
IS 4
AR 043303
DI 10.1063/1.4873175
PG 15
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA AH5FA
UT WOS:000336152700026
ER
PT J
AU Vogt, SS
Radovan, M
Kibrick, R
Butler, RP
Alcott, B
Allen, S
Arriagada, P
Bolte, M
Burt, J
Cabak, J
Chloros, K
Cowley, D
Deich, W
Dupraw, B
Earthman, W
Epps, H
Faber, S
Fischer, D
Gates, E
Hilyard, D
Holden, B
Johnston, K
Keiser, S
Kanto, D
Katsuki, M
Laiterman, L
Lanclos, K
Laughlin, G
Lewis, J
Lockwood, C
Lynam, P
Marcy, G
McLean, M
Miller, J
Misch, T
Peck, M
Pfister, T
Phillips, A
Rivera, E
Sandford, D
Saylor, M
Stover, R
Thompson, M
Walp, B
Ward, J
Wareham, J
Wei, MZ
Wright, C
AF Vogt, Steven S.
Radovan, Matthew
Kibrick, Robert
Butler, R. Paul
Alcott, Barry
Allen, Steve
Arriagada, Pamela
Bolte, Mike
Burt, Jennifer
Cabak, Jerry
Chloros, Kostas
Cowley, David
Deich, William
Dupraw, Brian
Earthman, Wayne
Epps, Harland
Faber, Sandra
Fischer, Debra
Gates, Elinor
Hilyard, David
Holden, Brad
Johnston, Ken
Keiser, Sandy
Kanto, Dick
Katsuki, Myra
Laiterman, Lee
Lanclos, Kyle
Laughlin, Greg
Lewis, Jeff
Lockwood, Chris
Lynam, Paul
Marcy, Geoffrey
McLean, Maureen
Miller, Joe
Misch, Tony
Peck, Michael
Pfister, Terry
Phillips, Andrew
Rivera, Eugenio
Sandford, Dale
Saylor, Mike
Stover, Richard
Thompson, Matthew
Walp, Bernie
Ward, James
Wareham, John
Wei, Mingzhi
Wright, Chris
TI APF-The Lick Observatory Automated Planet Finder
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID ECHELLE-SPECTROMETER; SPECTROGRAPH; TELESCOPE; FITS; REPRESENTATIONS;
SYSTEM; I.
AB The Automated Planet Finder (APF) is a facility purpose-built for the discovery and characterization of extrasolar planets through high-cadence Doppler velocimetry of the reflex barycentric accelerations of their host stars. Located atop Mount Hamilton, the APF facility consists of a 2.4 m telescope and its Levy spectrometer, an optical echelle spectrometer optimized for precision Doppler velocimetry. APP features a fixed-forivat spectral range from 374-970 nm, and delivers a "throughput" (resolution x slit width product) of 114,000", with spectral resolutions up to 150,000. Overall system efficiency (fraction of photons incident on the primary mirror that are detected by the science CCD) on blaze at 560 nm in planet-hunting mode is 15%. First-light tests on the radial-velocity (RV) standard stars HD 185144 and HD 9407 demonstrate sub-meter-per-second precision (rms per observation) held over a 3 month period. This paper reviews the basic features of the telescope, dome, and spectrometer, and gives a brief summary of first-light performance.
C1 [Vogt, Steven S.; Radovan, Matthew; Kibrick, Robert; Alcott, Barry; Allen, Steve; Bolte, Mike; Burt, Jennifer; Cabak, Jerry; Chloros, Kostas; Cowley, David; Deich, William; Dupraw, Brian; Earthman, Wayne; Epps, Harland; Faber, Sandra; Gates, Elinor; Hilyard, David; Holden, Brad; Kanto, Dick; Katsuki, Myra; Laiterman, Lee; Lanclos, Kyle; Laughlin, Greg; Lewis, Jeff; Lockwood, Chris; Lynam, Paul; McLean, Maureen; Miller, Joe; Misch, Tony; Peck, Michael; Pfister, Terry; Phillips, Andrew; Rivera, Eugenio; Sandford, Dale; Saylor, Mike; Stover, Richard; Thompson, Matthew; Ward, James; Wareham, John; Wei, Mingzhi; Wright, Chris] Univ Calif Santa Cruz, Univ Calif Observ, Santa Cruz, CA 95064 USA.
[Butler, R. Paul; Arriagada, Pamela; Keiser, Sandy] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Johnston, Ken] US Naval Observ, Washington, DC 20392 USA.
[Marcy, Geoffrey] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Walp, Bernie] NASA, Stratospher Observ Infrared Astron, Dryden Flight Res Ctr, Edwards AFB, CA 93523 USA.
RP Vogt, SS (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Santa Cruz, CA 95064 USA.
RI Butler, Robert/B-1125-2009
FU R-California; NASA [NAG5-13448]; NSF [AST-0307493]
FX We are deeply indebted to Congressman Jerry Lewis (R-California,
retired) for securing the Congressional earmark funding that formed the
cornerstone of this project Thanks to Andrew Gray and Ian Ritchie of
EOS, for their advice and assistance regarding APF telescope balance,
encoder alignment, and various other telescope and dome operational
procedures; to former EOST staff members Kevin Harris and Elwood Downey,
for their suggestions regarding APF servo tuning, and to Andrew Lowman,
for his advice regarding thermal compensation of M2 focus. We thank
Vilma and Dave Anderson of Rayleigh Optical for the superb job they did
on polishing and figuring the 2.4 m primary mirror. We are grateful to
Gillian Knave and Craig Sonsetti of NIST for providing the critical
high-resolution FT'S scans of the iodine cell. We would also like to
acknowledge the excellent coating work done for us by Ric Shimshock and
the folks at MLD Technologies LLC. We are especially grateful to Joe
Wampler, Phil Crane, and Anne Kinney of NASA for their critical infusion
of funds through NASA grant NAG5-13448 that funded the spectrometer and
allowed us to super-size APF from a 1.8 m to a 2.4 m. We are grateful to
Wayne Rosing of Las Cumbres Observatory for his donation of the 5-axis
mill which was used to fabricate the determinate structure nodes. We
especially would like to thank Ken and Gloria Levy for their generous
contribution that helped fund completion of the spectrometer, Geoff
Marcy and Susan Kegley for their personal contribution, and the Nick
Konidaris family for their generous contribution. Finally, we are most
grateful to the NSF for grant AST-0307493 that funded much of the
observing software and commissioning activities.
NR 28
TC 20
Z9 20
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD APR
PY 2014
VL 126
IS 938
BP 359
EP 379
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH5TK
UT WOS:000336193800005
ER
PT J
AU Howell, SB
Sobeck, C
Haas, M
Still, M
Barclay, T
Mullally, F
Troeltzsch, J
Aigrain, S
Bryson, ST
Caldwell, D
Chaplin, WJ
Cochran, WD
Huber, D
Marcy, GW
Miglio, A
Najita, JR
Smith, M
Twicken, JD
Fortney, JJ
AF Howell, Steve B.
Sobeck, Charlie
Haas, Michael
Still, Martin
Barclay, Thomas
Mullally, Fergal
Troeltzsch, John
Aigrain, Suzanne
Bryson, Stephen T.
Caldwell, Doug
Chaplin, William J.
Cochran, William D.
Huber, Daniel
Marcy, Geoffrey W.
Miglio, Andrea
Najita, Joan R.
Smith, Marcie
Twicken, J. D.
Fortney, Jonathan J.
TI The K2 Mission: Characterization and Early Results
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID RAPID OPTICAL VARIABILITY; ACTIVE GALACTIC NUCLEI; RED-GIANT STARS;
MICROLENS PARALLAXES; STELLAR POPULATIONS; KEPLER OBSERVATIONS;
PLANETARY SYSTEMS; LIGHT CURVES; SOLAR-TYPE; X-RAY
AB The K2 mission will make use of the Kepler spacecraft and its assets to expand upon Kepler's groundbreaking discoveries in the fields of exoplanets and astrophysics through new and exciting observations. K2 will use an innovative way of operating the spacecraft to observe target fields along the ecliptic for the next 2-3 years. Early science commissioning observations have shown an estimated photometric precision near 400 ppm in a single 30 minute observation, and a 6-hr photometric precision of 80 ppm (both at V = 12). The K2 mission offers long-term, simultaneous optical observation of thousands of objects at a precision far better than is achievable from ground-based telescopes. Ecliptic fields will be observed for approximately 75 days enabling a unique exoplanet survey which fills the gaps in duration and sensitivity between the Kepler and TESS missions, and offers prelaunch exoplanet target identification for JWST transit spectroscopy. Astrophysics observations with K2 will include studies of young open clusters, bright stars, galaxies, supernovae, and asteroseismology.
C1 [Howell, Steve B.; Sobeck, Charlie; Haas, Michael; Still, Martin; Barclay, Thomas; Mullally, Fergal; Bryson, Stephen T.; Caldwell, Doug; Huber, Daniel; Smith, Marcie; Twicken, J. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Still, Martin; Barclay, Thomas] Bay Area Environm Res Inst, West Sonoma, CA 95476 USA.
[Mullally, Fergal; Caldwell, Doug; Huber, Daniel; Smith, Marcie; Twicken, J. D.] SETI Inst, Mountain View, CA 94043 USA.
[Troeltzsch, John] Ball Aerosp & Technol Corp, Boulder, CO 80306 USA.
[Aigrain, Suzanne] Univ Oxford, Dept Phys, Subdept Astrophys, Oxford OX1 3RH, England.
[Chaplin, William J.; Miglio, Andrea] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Chaplin, William J.; Miglio, Andrea] Aarhus Univ, SAC, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Marcy, Geoffrey W.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Najita, Joan R.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
RP Howell, SB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RI Caldwell, Douglas/L-7911-2014
OI Caldwell, Douglas/0000-0003-1963-9616
NR 64
TC 272
Z9 272
U1 2
U2 10
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD APR
PY 2014
VL 126
IS 938
BP 398
EP 408
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AH5TK
UT WOS:000336193800008
ER
PT J
AU Slaba, TC
Blattnig, SR
AF Slaba, Tony C.
Blattnig, Steve R.
TI GCR environmental models I: Sensitivity analysis for GCR environments
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE galactic cosmic rays; space radiation; uncertainty quantification
ID ADVANCED COMPOSITION EXPLORER; COSMIC-RAY MODEL; RADIATION PROTECTION;
SPACE RADIATION; EXPOSURE; HZETRN
AB Accurate galactic cosmic ray (GCR) models are required to assess crew exposure during long-duration missions to the Moon or Mars. Many of these models have been developed and compared to available measurements, with uncertainty estimates usually stated to be less than 15%. However, when the models are evaluated over a common epoch and propagated through to effective dose, relative differences exceeding 50% are observed. This indicates that the metrics used to communicate GCR model uncertainty can be better tied to exposure quantities of interest for shielding applications. This is the first of three papers focused on addressing this need. In this work, the focus is on quantifying the extent to which each GCR ion and energy group, prior to entering any shielding material or body tissue, contributes to effective dose behind shielding. Results can be used to more accurately calibrate model-free parameters and provide a mechanism for refocusing validation efforts on measurements taken over important energy regions. Results can also be used as references to guide future nuclear cross-section measurements and radiobiology experiments. It is found that GCR with Z>2 and boundary energies below 500MeV/n induce less than 5% of the total effective dose behind shielding. This finding is important given that most of the GCR models are developed and validated against Advanced Composition Explorer/Cosmic Ray Isotope Spectrometer (ACE/CRIS) measurements taken below 500MeV/n. It is therefore possible for two models to very accurately reproduce the ACE/CRIS data while inducing very different effective dose values behind shielding.
Key Points
GCR model uncertainty may be higher than 15% GCR ions below 500 MeV/n contribute less than 5% to effective dose ACE/CRIS measurements induce less than 5% of effective dose
C1 [Slaba, Tony C.; Blattnig, Steve R.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Slaba, TC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM tony.c.slaba@nasa.gov
FU Human Research Program under the Human Exploration and Operations
Mission Directorate of NASA
FX This work was supported by the Human Research Program under the Human
Exploration and Operations Mission Directorate of NASA. The authors
would like to thank Pat O'Neill for providing the BON2011 source code.
The data presented in this paper may be obtained by contacting the
authors.
NR 26
TC 7
Z9 7
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD APR
PY 2014
VL 12
IS 4
BP 217
EP 224
DI 10.1002/2013SW001025
PG 8
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA AG9IE
UT WOS:000335731800004
ER
PT J
AU Slaba, TC
Blattnig, SR
AF Slaba, Tony C.
Blattnig, Steve R.
TI GCR environmental models II: Uncertainty propagation methods for GCR
environments
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE space radiation; galactic cosmic rays; uncertainty quantification
ID ADVANCED COMPOSITION EXPLORER; RADIATION; HZETRN
AB In order to assess the astronaut exposure received within vehicles or habitats, accurate models of the ambient galactic cosmic ray (GCR) environment are required. Many models have been developed and compared to measurements, with uncertainty estimates often stated to be within 15%. However, intercode comparisons can lead to differences in effective dose exceeding 50%. This is the second of three papers focused on resolving this discrepancy. The first paper showed that GCR heavy ions with boundary energies below 500 MeV/n induce less than 5% of the total effective dose behind shielding. Yet, due to limitations on available data, model development and validation are heavily influenced by comparisons to measurements taken below 500 MeV/n. In the current work, the focus is on developing an efficient method for propagating uncertainties in the ambient GCR environment to effective dose values behind shielding. A simple approach utilizing sensitivity results from the first paper is described and shown to be equivalent to a computationally expensive Monte Carlo uncertainty propagation. The simple approach allows a full uncertainty propagation to be performed once GCR uncertainty distributions are established. This rapid analysis capability may be integrated into broader probabilistic radiation shielding analysis and also allows error bars (representing boundary condition uncertainty) to be placed around point estimates of effective dose.
Key Points
Sensitivity results can be used to propagate uncertainties Fast method developed for propagating boundary condition uncertainties GCR ions with E<500 MeV/n have small impact on effective dose
C1 [Slaba, Tony C.; Blattnig, Steve R.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Slaba, TC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM tony.c.slaba@nasa.gov
FU Human Research Program under the Human Exploration and Operations
Mission Directorate of NASA
FX This work was supported by the Human Research Program under the Human
Exploration and Operations Mission Directorate of NASA. The data
presented in this paper may be obtained by contacting the authors.
NR 20
TC 4
Z9 4
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD APR
PY 2014
VL 12
IS 4
BP 225
EP 232
DI 10.1002/2013SW001026
PG 8
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA AG9IE
UT WOS:000335731800005
ER
PT J
AU Slaba, TC
Xu, XJ
Blattnig, SR
Norman, RB
AF Slaba, Tony C.
Xu, Xiaojing
Blattnig, Steve R.
Norman, Ryan B.
TI GCR environmental models III: GCR model validation and propagated
uncertainties in effective dose
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE Space Radiation; Galactic Cosmic Rays; Uncertainty Quantification
ID COSMIC-RAY PROTON; ADVANCED COMPOSITION EXPLORER; ENERGY-SPECTRA; HELIUM
SPECTRA; CHARGE COMPOSITION; NUCLEI; RADIATION; SPACE
AB This is the last of three papers focused on quantifying the uncertainty associated with galactic cosmic rays (GCR) models used for space radiation shielding applications. In the first paper, it was found that GCR ions with Z>2 and boundary energy below 500MeV/nucleon induce less than 5% of the total effective dose behind shielding. This is an important finding since GCR model development and validation have been heavily biased toward Advanced Composition Explorer/Cosmic Ray Isotope Spectrometer measurements below 500MeV/nucleon. Weights were also developed that quantify the relative contribution of defined GCR energy and charge groups to effective dose behind shielding. In the second paper, it was shown that these weights could be used to efficiently propagate GCR model uncertainties into effective dose behind shielding. In this work, uncertainties are quantified for a few commonly used GCR models. A validation metric is developed that accounts for measurements uncertainty, and the metric is coupled to the fast uncertainty propagation method. For this work, the Badhwar-O'Neill (BON) 2010 and 2011 and the Matthia GCR models are compared to an extensive measurement database. It is shown that BON2011 systematically overestimates heavy ion fluxes in the range 0.5-4GeV/nucleon. The BON2010 and BON2011 also show moderate and large errors in reproducing past solar activity near the 2000 solar maximum and 2010 solar minimum. It is found that all three models induce relative errors in effective dose in the interval [-20%, 20%] at a 68% confidence level. The BON2010 and Matthia models are found to have similar overall uncertainty estimates and are preferred for space radiation shielding applications.
Key Points
BON2011 over estimates heavy ion flux at relevant energies BON2010 and Matthia models have similar overall uncertainty statements GCR model uncertainty may be reduced by calibrating to high energy data
C1 [Slaba, Tony C.; Blattnig, Steve R.; Norman, Ryan B.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Xu, Xiaojing] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Slaba, TC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM tony.c.slaba@nasa.gov
RI Norman, Ryan/D-5095-2017
OI Norman, Ryan/0000-0002-9103-7225
FU Human Research Program under the Human Exploration and Operations
Mission Directorate of NASA; NASA [NNL11AA00B]
FX This work was supported by the Human Research Program under the Human
Exploration and Operations Mission Directorate of NASA and by NASA grant
NNL11AA00B. The authors would like to thank Pat O'Neill for providing
the BON2011 source code and Daniel Matthia for providing the Matthia
source code. The data presented in this paper may be obtained by
contacting the authors.
NR 41
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U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD APR
PY 2014
VL 12
IS 4
BP 233
EP 245
DI 10.1002/2013SW001027
PG 13
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA AG9IE
UT WOS:000335731800006
ER
PT J
AU Kim, RS
Moon, YJ
Gopalswamy, N
Park, YD
Kim, YH
AF Kim, R. -S.
Moon, Y. -J.
Gopalswamy, N.
Park, Y. -D.
Kim, Y. -H.
TI Two-step forecast of geomagnetic storm using coronal mass ejection and
solar wind condition
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE geomagnetic storm forecast; coronal mass ejection; solar wind
ID CME EARTHWARD DIRECTION; INTERPLANETARY SHOCK; HALO CMES; MAGNETIC
STORMS; RING CURRENT; ART.; GEOEFFECTIVENESS; PARAMETERS; MODEL; DST
AB To forecast geomagnetic storms, we had examined initially observed parameters of coronal mass ejections (CMEs) and introduced an empirical storm forecast model in a previous study. Now we suggest a two-step forecast considering not only CME parameters observed in the solar vicinity but also solar wind conditions near Earth to improve the forecast capability. We consider the empirical solar wind criteria derived in this study (B-z-5 nT or E-y 3 mV/m for t 2 h for moderate storms with minimum Dst less than -50 nT) and a Dst model developed by Temerin and Li (2002, 2006) (TL model). Using 55 CME-Dst pairs during 1997 to 2003, our solar wind criteria produce slightly better forecasts for 31 storm events (90%) than the forecasts based on the TL model (87%). However, the latter produces better forecasts for 24 nonstorm events (88%), while the former correctly forecasts only 71% of them. We then performed the two-step forecast. The results are as follows: (i) for 15 events that are incorrectly forecasted using CME parameters, 12 cases (80%) can be properly predicted based on solar wind conditions; (ii) if we forecast a storm when both CME and solar wind conditions are satisfied (), the critical success index becomes higher than that from the forecast using CME parameters alone, however, only 25 storm events (81%) are correctly forecasted; and (iii) if we forecast a storm when either set of these conditions is satisfied (), all geomagnetic storms are correctly forecasted.
Key Points This study is for the improvement of empirical geomagnetic storm forecast We use the initially observed CME parameters as the first-step of the forecast We also use the solar wind parameters for near-real forecast
C1 [Kim, R. -S.; Park, Y. -D.; Kim, Y. -H.] Korea Astron & Space Sci Inst, Astron & Space Program Div, Taejon, South Korea.
[Moon, Y. -J.] Kyung Hee Univ, Sch Space Res, Yongin, South Korea.
[Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD 20771 USA.
RP Kim, RS (reprint author), Korea Astron & Space Sci Inst, Astron & Space Program Div, Taejon, South Korea.
EM rskim@kasi.re.kr
RI Moon, Yong-Jae/E-1711-2013;
OI Gopalswamy, Nat/0000-0001-5894-9954
FU Construction of Korean Space Weather Center as the project of KASI; KASI
Basic Research Fund; Research Fellowship for Young Scientists of KRCF;
WCU program [R31-10016]; Basic Research Promotion Fund through the
National Research Foundation of Korea - Ministry of Education, Science,
and Technology [20090071744, 20100014501]
FX We thank the referees for careful reading of the manuscript and valuable
suggestions and criticism that led to significant improvement of the
paper. This work was supported by the Construction of Korean Space
Weather Center as the project of KASI, the KASI Basic Research Fund, and
Research Fellowship for Young Scientists of KRCF. Y.-J.M. has been
supported by the WCU program (R31-10016) and Basic Research Promotion
Fund (20090071744 and 20100014501) through the National Research
Foundation of Korea funded by the Ministry of Education, Science, and
Technology.
NR 39
TC 2
Z9 2
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD APR
PY 2014
VL 12
IS 4
BP 246
EP 256
DI 10.1002/2014SW001033
PG 11
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA AG9IE
UT WOS:000335731800007
ER
PT J
AU Posner, A
Hesse, M
St Cyr, OC
AF Posner, A.
Hesse, M.
St Cyr, O. C.
TI The main pillar: Assessment of space weather observational asset
performance supporting nowcasting, forecasting, and research to
operations
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE SWx Forecasting; Space Hardware; Assessment
ID INTERPLANETARY MAGNETIC-FIELD; CORONAL MASS EJECTIONS; ADVANCED
COMPOSITION EXPLORER; EARTH CONNECTION EVENTS; 29-31 OCTOBER 2003;
SOLAR-WIND; GEOMAGNETIC STORMS; ENERGETIC PARTICLES; ARRIVAL TIMES;
PROPAGATION
AB Space weather forecasting critically depends upon availability of timely and reliable observational data. It is therefore particularly important to understand how existing and newly planned observational assets perform during periods of severe space weather. Extreme space weather creates challenging conditions under which instrumentation and spacecraft may be impeded or in which parameters reach values that are outside the nominal observational range. This paper analyzes existing and upcoming observational capabilities for forecasting, and discusses how the findings may impact space weather research and its transition to operations. A single limitation to the assessment is lack of information provided to us on radiation monitor performance, which caused us not to fully assess (i.e., not assess short term) radiation storm forecasting. The assessment finds that at least two widely spaced coronagraphs including L4 would provide reliability for Earth-bound CMEs. Furthermore, all magnetic field measurements assessed fully meet requirements. However, with current or even with near term new assets in place, in the worst-case scenario there could be a near-complete lack of key near-real-time solar wind plasma data of severe disturbances heading toward and impacting Earth's magnetosphere. Models that attempt to simulate the effects of these disturbances in near real time or with archival data require solar wind plasma observations as input. Moreover, the study finds that near-future observational assets will be less capable of advancing the understanding of extreme geomagnetic disturbances at Earth, which might make the resulting space weather models unsuitable for transition to operations.
Key Points
Manuscript assesses current and near-future space weather assets Current assets unreliable for forecasting of severe geomagnetic storms Near-future assets will not improve the situation
C1 [Posner, A.; Hesse, M.; St Cyr, O. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Posner, A.] NASA Headquarters, Washington, DC USA.
RP Posner, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM arik.posner@nasa.gov
OI Posner, Arik/0000-0003-1572-8734
FU NASA
FX The authors gratefully acknowledge the support provided by the NASA
mission and instrument teams in 2011 and helpful suggestions provided by
the reviewers of the manuscript in 2012 and 2013. We also acknowledge
the anonymous NOAA review provided to us in early 2013.
NR 92
TC 3
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U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD APR
PY 2014
VL 12
IS 4
BP 257
EP 276
DI 10.1002/2013SW001007
PG 20
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA AG9IE
UT WOS:000335731800008
ER
PT J
AU Cotton, MM
Bruhn, RL
Sauber, J
Burgess, E
Forster, RR
AF Cotton, Michelle M.
Bruhn, Ronald L.
Sauber, Jeanne
Burgess, Evan
Forster, Richard R.
TI Ice surface morphology and flow on Malaspina Glacier, Alaska:
Implications for regional tectonics in the Saint Elias orogen
SO TECTONICS
LA English
DT Article
DE tectonics; glaciers; remote sensing; Saint Elias; Alaska; Yakutat
ID GROUND DEFORMATION MEASUREMENTS; 1979 ST-ELIAS; ELEVATION CHANGES;
SOUTHERN ALASKA; CANADA; USA; TERRANE; THRUST; SYSTEM; IMAGES
AB The Saint Elias Mountains in southern Alaska are located at a structural syntaxis where the coastal thrust and fold belt of the Fairweather plate boundary intersects thrust faults and folds generated by collision of the Yakutat Terrane. The axial trace of this syntaxis extends southeastward out of the Saint Elias Mountains and beneath Malaspina Glacier where it is hidden from view and cannot be mapped using conventional methods. Here we examine the surface morphology and flow patterns of Malaspina Glacier to infer characteristics of the bedrock topography and organization of the syntaxis. Faults and folds beneath the eastern part of the glacier trend northwest and reflect dextral transpression near the terminus of the Fairweather fault system. Those beneath the western part of the glacier trend northeast and accommodate folding and thrust faulting during collision and accretion of the Yakutat Terrane. Mapping the location and geometry of the structural syntaxis provides important constraints on spatial variations in seismicity, fault kinematics, and crustal shortening beneath Malaspina Glacier, as well as the position of the collisional deformation front within the Yakutat Terrane. We also speculate that the geometrical complexity of intersecting faults within the syntaxis formed a barrier to rupture propagation during two regional Mw 8.1 earthquakes in September 1899.
Key Points Structural domains of Malaspina Glacier Glacial morphology and flow reflect basal topography and structural geology Feature tracking of ice velocities on Malaspina Glacier
C1 [Cotton, Michelle M.; Bruhn, Ronald L.] Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA.
[Sauber, Jeanne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Burgess, Evan; Forster, Richard R.] Univ Utah, Dept Geog, Salt Lake City, UT USA.
RP Cotton, MM (reprint author), Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA.
EM michellemariecotton@gmail.com
FU National Aeronautics and Space Administration (NASA) [NNX08AX88G]; NASA
Science Innovation Fund at Goddard Space Flight Center; NASA Earth
Science Space Fellowship; NASA [NNX08AP27G]
FX National Aeronautics and Space Administration (NASA) grant entitled
"Geodetic Imaging of Glacioseismotectonic Processes in Southern Alaska"
(NNX08AX88G) awarded to J. Sauber, R. R. Forster, and R. L. Bruhn
supported this research. J. Sauber was also supported by funding from
the NASA 2012 Science Innovation Fund at Goddard Space Flight Center. E.
Burgess was funded under the NASA Earth Science Space Fellowship. E.
Burgess and R. R. Forster were also partially supported by NASA grant
NNX08AP27G. We thank the editors at Tectonics and those who reviewed the
manuscript, J. B. Chapman and L. Stearns, for their input and help.
NR 45
TC 2
Z9 2
U1 3
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0278-7407
EI 1944-9194
J9 TECTONICS
JI Tectonics
PD APR
PY 2014
VL 33
IS 4
BP 581
EP 595
DI 10.1002/2013TC003381
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AH6PT
UT WOS:000336253800011
ER
PT J
AU Thurlow, ME
Co, DT
O'Brien, AS
Hannun, RA
Lapson, LB
Hanisco, TF
Anderson, JG
AF Thurlow, M. E.
Co, D. T.
O'Brien, A. S.
Hannun, R. A.
Lapson, L. B.
Hanisco, T. F.
Anderson, J. G.
TI The development and deployment of a ground-based, laser-induced
fluorescence instrument for the in situ detection of iodine monoxide
radicals
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID MARINE BOUNDARY-LAYER; LOWER STRATOSPHERE; POTENTIAL INFLUENCE; RATE
COEFFICIENTS; MOLECULAR-IODINE; FREE TROPOSPHERE; REACTIVE IODINE;
EASTERN PACIFIC; OZONE DEPLETION; GASEOUS IODINE
AB High abundances of iodine monoxide (IO) are known to exist and to participate in local photochemistry of the marine boundary layer. Of particular interest are the roles IO plays in the formation of new particles in coastal marine environments and in depletion episodes of ozone and mercury in the Arctic polar spring. This paper describes a ground-based instrument that measures IO at mixing ratios less than one part in 10(12). The IO radical is measured by detecting laser-induced fluorescence at wavelengths longer that 500 nm. Tunable visible light is used to pump the A(2)Pi(3/2) (v' = 2) <- X-2 Pi(3/2) (v '' = 0) transition of IO near 445 nm. The laser light is produced by a solid-state, Nd: YAG-pumped Ti:Sapphire laser at 5 kHz repetition rate. The laser-induced fluorescence instrument performs reliably with very high signal-to-noise ratios (> 10) achieved in short integration times (< 1 min). The observations from a validation deployment to the Shoals Marine Lab on Appledore Island, ME are presented and are broadly consistent with in situ observations from European Coastal Sites. Mixing ratios ranged from the instrumental detection limit (< 1 pptv) to 10 pptv. These data represent the first in situ point measurements of IO in North America. (C) 2014 AIP Publishing LLC.
C1 [Thurlow, M. E.; Co, D. T.; O'Brien, A. S.; Hannun, R. A.; Lapson, L. B.; Hanisco, T. F.; Anderson, J. G.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA.
[Co, D. T.] Northwestern Univ, Argonne Northwestern Solar Energy Res Ctr, Evanston, IL 60208 USA.
[Co, D. T.] Northwestern Univ, Dept Chem, Evanston, IL 60208 USA.
[O'Brien, A. S.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
[Hanisco, T. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Thurlow, ME (reprint author), Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA.
EM thurlow@huarp.harvard.edu
FU National Science Foundation [0733875]
FX The authors wish to thank Norton Allen, Joe Demusz, Mike Greenberg, Matt
Knight, Terry Martin, Danny Spillane, Ed Thomspon, and Chris Tuozzolo
for engineering support. M. T. wishes to thank the staff of the Shoals
Marine Laboratory and Charles Praska for logistical assistance and
Steven Wofsy and Roisin Commane for technical advice. This work was
supported by the National Science Foundation (Award No.: 0733875).
NR 83
TC 0
Z9 0
U1 1
U2 17
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0034-6748
EI 1089-7623
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD APR
PY 2014
VL 85
IS 4
AR 044101
DI 10.1063/1.4869857
PG 14
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA AH1ZN
UT WOS:000335920600043
PM 24784629
ER
PT J
AU Wollack, EJ
Kinzer, RE
Rinehart, SA
AF Wollack, E. J.
Kinzer, R. E., Jr.
Rinehart, S. A.
TI A cryogenic infrared calibration target
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID LIGHT TRAP; DESIGN; SUBMILLIMETER; REFLECTANCE; ABSORBER; REGION
AB A compact cryogenic calibration target is presented that has a peak diffuse reflectance, R <= 0.003, from 800 to 4800 cm(-1) (12 - 2 mu m). Upon expanding the spectral range under consideration to 400-10 000 cm(-1) (25 - 1 mu m) the observed performance gracefully degrades to R <= 0.02 at the band edges. In the implementation described, a high-thermal-conductivity metallic substrate is textured with a pyramidal tiling and subsequently coated with a thin lossy dielectric coating that enables high absorption and thermal uniformity across the target. The resulting target assembly is lightweight, has a low-geometric profile, and has survived repeated thermal cycling from room temperature to similar to 4 K. Basic design considerations, governing equations, and test data for realizing the structure described are provided. The optical properties of selected absorptive materials-Acktar Fractal Black, Aeroglaze Z306, and Stycast 2850 FT epoxy loaded with stainless steel powder-are characterized and presented.
C1 [Wollack, E. J.; Kinzer, R. E., Jr.; Rinehart, S. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wollack, EJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM edward.j.wollack@nasa.gov
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
FU NASA ROSES/APRA program
FX The authors gratefully acknowledge financial support from the NASA
ROSES/APRA program and thank E. Sharp and C. Wheeler for their
contributions to preparation and fabrication of the structures presented
here. R. Kinzer was supported by an appointment to the NASA Postdoctoral
Program at GSFC, administered by the Oak Ridge Associated Universities.
NR 33
TC 4
Z9 4
U1 1
U2 7
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0034-6748
EI 1089-7623
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD APR
PY 2014
VL 85
IS 4
AR 044707
DI 10.1063/1.4871108
PG 5
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA AH1ZN
UT WOS:000335920600052
PM 24784638
ER
PT J
AU Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Blandford, RD
Borgland, AW
Bregeon, J
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Cavazzuti, E
Cecchi, C
Chaves, RCG
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
D'Ammando, F
de Angelis, A
Dermer, CD
Digel, SW
Silva, EDE
Drell, PS
Drlica-Wagner, A
Favuzzi, C
Focke, WB
Franckowiak, A
Fukazawa, Y
Fusco, P
Gargano, F
Gasparrini, D
Germani, S
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grove, JE
Guiriec, S
Hadasch, D
Hayashida, M
Hays, E
Hughes, RE
Jackson, MS
Jogler, T
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Mazziotta, MN
Mehault, J
Michelson, PF
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nemmen, R
Nuss, E
Ohsugi, T
Omodei, N
Orienti, M
Orlando, E
Paneque, D
Perkins, JS
Piron, F
Pivato, G
Prokhorov, D
Raino, S
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Ritz, S
Romoli, C
Sanchez-Conde, M
Sanchez, DA
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Takahashi, H
Tanaka, T
Tibaldo, L
Tinivella, M
Tosti, G
Troja, E
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Winer, BL
Wood, KS
Yang, Z
AF Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Blandford, R. D.
Borgland, A. W.
Bregeon, J.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Cavazzuti, E.
Cecchi, C.
Chaves, R. C. G.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
D'Ammando, F.
de Angelis, A.
Dermer, C. D.
Digel, S. W.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Favuzzi, C.
Focke, W. B.
Franckowiak, A.
Fukazawa, Y.
Fusco, P.
Gargano, F.
Gasparrini, D.
Germani, S.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Hadasch, D.
Hayashida, M.
Hays, E.
Hughes, R. E.
Jackson, M. S.
Jogler, T.
Knoedlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Mazziotta, M. N.
Mehault, J.
Michelson, P. F.
Mizuno, T.
Moiseev, A. A.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nemmen, R.
Nuss, E.
Ohsugi, T.
Omodei, N.
Orienti, M.
Orlando, E.
Paneque, D.
Perkins, J. S.
Piron, F.
Pivato, G.
Prokhorov, D.
Raino, S.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Ritz, S.
Romoli, C.
Sanchez-Conde, M.
Sanchez, D. A.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Takahashi, H.
Tanaka, T.
Tibaldo, L.
Tinivella, M.
Tosti, G.
Troja, E.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Winer, B. L.
Wood, K. S.
Yang, Z.
TI Fermi LARGE AREA TELESCOPE OBSERVATIONS OF BLAZAR 3C 279 OCCULTATIONS BY
THE SUN
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astroparticle physics; gamma rays: general; occultations; quasars:
individual (3C 279); Sun: X-rays, gamma rays
ID ACTIVE GALACTIC NUCLEI; GAMMA-RAY EMISSION; MAGNETIC-FIELDS; PAIR HALOS;
EGRET DATA; CONSEQUENCES; PHOTON; AXION
AB Observations of occultations of bright. gamma-ray sources by the Sun may reveal predicted pair halos around blazars and/or new physics, such as, e.g., hypothetical light dark matter particles-axions. We use Fermi Gamma-Ray Space Telescope (Fermi) data to analyze four occultations of blazar 3C 279 by the Sun on October 8 each year from 2008 to 2011. A combined analysis of the observations of these occultations allows a point-like source at the position of 3C 279 to be detected with significance of approximate to 3 sigma, but does not reveal any significant excess over the flux expected from the quiescent Sun. The likelihood ratio test rules out complete transparency of the Sun to the blazar. gamma-ray emission at a 3s confidence level.
C1 [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.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.; Romoli, C.; Tibaldo, L.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Prokhorov, D.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Tanaka, T.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Prokhorov, D.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Tanaka, T.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Bellazzini, R.; Bregeon, J.; Kuss, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bruel, P.] Ecole Polytech, CNRS IN2P3, Lab Leprince Ringuet, Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Gasparrini, D.; Giommi, P.] ASI Sci Data Ctr, I-00044 Rome, Italy.
[Cecchi, C.; D'Ammando, F.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA IRFU CNRS, F-91191 Gif Sur Yvette, France.
[Cheung, C. C.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS IN2P3, Lab Univers & Particules Montpellier, Montpellier, France.
[D'Ammando, F.; Mehault, J.] IASF Palermo, I-90146 Palermo, Italy.
[Chekhtman, A.; D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Grp Coll Udine, Ist Nazl Fis Nucl, Sez Trieste, I-33100 Udine, Italy.
[Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[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.
[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.
[Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.; Hays, E.; Nemmen, R.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Jackson, M. S.] Royal Inst Technol KTH, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
[Jackson, M. S.; Larsson, S.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Knoedlseder, J.; Yang, Z.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France.
[Larsson, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Moiseev, A. A.; Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA.
[Moiseev, A. A.; Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[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.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Vianello, G.] CIFS, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RP Barbiellini, G (reprint author), Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
EM imos@stanford.edu; phdmitry@stanford.edu
RI Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen,
Rodrigo/O-6841-2014; Loparco, Francesco/O-8847-2015; Mazziotta, Mario
/O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012;
Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Orlando,
E/R-5594-2016;
OI Reimer, Olaf/0000-0001-6953-1385; Caraveo, Patrizia/0000-0003-2478-8018;
Morselli, Aldo/0000-0002-7704-9553; Loparco,
Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672;
Gargano, Fabio/0000-0002-5055-6395; giglietto,
nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X;
Giordano, Francesco/0000-0002-8651-2394; giommi,
paolo/0000-0002-2265-5003; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI,
Paolo/0000-0001-6688-8864; Bastieri, Denis/0000-0002-6954-8862; orienti,
monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852;
Gasparrini, Dario/0000-0002-5064-9495
NR 24
TC 4
Z9 4
U1 1
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2014
VL 784
IS 2
AR 118
DI 10.1088/0004-637X/784/2/118
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400033
ER
PT J
AU Burlaga, LF
Ness, NF
AF Burlaga, L. F.
Ness, N. F.
TI VOYAGER 1 OBSERVATIONS OF THE INTERSTELLAR MAGNETIC FIELD AND THE
TRANSITION FROM THE HELIOSHEATH
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Cosmic rays; ISM: magnetic fields; solar wind; Sun: heliosphere
ID GALACTIC COSMIC-RAYS; OUTER HELIOSPHERE; TERMINATION SHOCK; STRENGTH
FLUCTUATIONS; RADIO-EMISSION; SOLAR ROTATION; HELIOPAUSE;
INTERPLANETARY; REGION; PLASMA
AB Voyager 1 (V1) has been observing interstellar magnetic fields for more than one year beginning approximate to 2012/209, when V1 crossed a current sheet, a "CS0" having the structure of a tangential discontinuity. The inclination of this current sheet is consistent with an interstellar magnetic field B draped on a blunt heliopause. Two other current sheets (sector boundaries) were observed at approximate to 2012/167 and approximate to 2011/276 with high inclinations (99 degrees +/- 10 degrees. and 89 degrees +/- 10 degrees, respectively). From 2013.0 to approximate to 2013.6, the difference between the azimuthal angle lambda of B from the Parker spiral angle at the latitude 34 degrees.6 of V1 was lambda - lambda(P) = 22 degrees +/- 3 degrees and the corresponding difference of the elevation angle delta was delta - delta(P) = 23 degrees +/- 8 degrees. During 2012, the deviation from the Parker spiral angle was somewhat smaller. The interstellar magnetic field has a "west to east polarity," opposite to the direction of planetary motions. The magnitude of B varied smoothly in the range 0.38-0.59 nT with an average B = 0.486 +/- 0.045 after 2012/237.7. The transition from heliosheath to interstellar magnetic fields is related to a "two-step" increase in the cosmic ray intensity observed by V1 from approximate to 2012.30 to approximate to 2012.65. The first step increase began near the end of an unusual "away-polarity" sector, and it reached a plateau when V1 moved into a "toward-polarity" sector that ended at CS0. The second step increase began slowly after V1 crossed CS0, and it ended abruptly at 2012/237.728.
C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA.
EM lburlagahsp@verizon.net; nfnudel@yahoo.com
NR 45
TC 38
Z9 39
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2014
VL 784
IS 2
AR 146
DI 10.1088/0004-637X/784/2/146
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400061
ER
PT J
AU Cannon, BE
Smith, CW
Isenberg, PA
Vasquez, BJ
Murphy, N
Nuno, RG
AF Cannon, Bradford E.
Smith, Charles W.
Isenberg, Philip A.
Vasquez, Bernard J.
Murphy, Neil
Nuno, Raquel G.
TI ULYSSES OBSERVATIONS OF MAGNETIC WAVES DUE TO NEWBORN INTERSTELLAR
PICKUP IONS. I. NEW OBSERVATIONS AND LINEAR ANALYSIS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instabilities; magnetic fields; solar wind; Sun: heliosphere; waves
ID DISTANT SOLAR-WIND; OUTER HELIOSPHERE; TERMINATION SHOCK; PROTONS;
TURBULENCE; HYDROGEN; EVOLUTION; ENERGY; SYSTEM; FIELD
AB We have examined Ulysses magnetic field data using dynamic spectrogram techniques that compute wave amplitude, polarization, and direction of propagation over a broad range of frequencies and time. Events were identified that showed a strong polarization signature and an enhancement of power above the local proton gyrofrequency. We perform a statistical study of 502 wave events in an effort to determine when, where, and why they are observed. Most notably, we find that waves arising from newborn interstellar pickup ions are relatively rare and difficult to find. The quantities normally employed in theories of wave growth are neutral atom density and quantities related to their ionization and the subsequent dynamics such as wind speed, solar wind flux, and magnetic field orientation. We find the observations of waves to be largely uncorrelated to these quantities except for mean field direction where quasi-radial magnetic fields are favored and solar wind proton flux where wave observations appear to be favored by low flux conditions which runs contrary to theoretical expectations of wave generation. It would appear that an explanation based on source physics and instability growth rates alone is not adequate to account for the times when these waves are seen.
C1 [Cannon, Bradford E.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA.
[Smith, Charles W.; Isenberg, Philip A.; Vasquez, Bernard J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Dept Phys, Durham, NH 03824 USA.
[Smith, Charles W.; Isenberg, Philip A.; Vasquez, Bernard J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Ctr Space Sci, Durham, NH 03824 USA.
[Murphy, Neil] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Nuno, Raquel G.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
RP Cannon, BE (reprint author), Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA.
EM bc13h@my.fsu.edu; Charles.Smith@unh.edu; Phil.Isenberg@unh.edu;
Bernie.Vasquez@unh.edu; Neil.Murphy@jpl.nasa.gov; raquel.nuno@asu.edu
FU NASA Guest Investigator [NNX07AH75G]; NSF [ATM0635863, AGS0962506];
Caltech [44A1085631]; NASA [NNX13AF97G, NNX11AJ37G]; NASA Space Grant
program
FX This work was supported in part by NASA Guest Investigator grant
NNX07AH75G and NSF grant ATM0635863. C.W.S. is supported by Caltech
subcontract 44A1085631 to the University of New Hampshire in support of
the ACE/MAG instrument. Part of the ACE mandate is to better understand
the role of pickup ions in the heliosphere. P.A.I. and B.J.V. are
supported by NASA grants NNX13AF97G and NNX11AJ37G as well as NSF grant
AGS0962506. B.E.C. was an undergraduate physics major working within the
Space Science Center at the time this work was performed and worked as
an undergraduate intern at JPL during the summer of 2012, supported by
the NASA Space Grant program. Portions of this research were carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
NR 40
TC 9
Z9 9
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2014
VL 784
IS 2
AR 150
DI 10.1088/0004-637X/784/2/150
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400065
ER
PT J
AU Duchene, G
Arriaga, P
Wyatt, M
Kennedy, G
Sibthorpe, B
Lisse, C
Holland, W
Wisniewski, J
Clampin, M
Kalas, P
Pinte, C
Wilner, D
Booth, M
Horner, J
Matthews, B
Greaves, J
AF Duchene, G.
Arriaga, P.
Wyatt, M.
Kennedy, G.
Sibthorpe, B.
Lisse, C.
Holland, W.
Wisniewski, J.
Clampin, M.
Kalas, P.
Pinte, C.
Wilner, D.
Booth, M.
Horner, J.
Matthews, B.
Greaves, J.
TI SPATIALLY RESOLVED IMAGING OF THE TWO-COMPONENT eta Crv DEBRIS DISK WITH
HERSCHEL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems; stars: individual (eta Crv)
ID SUN-LIKE STARS; TERRESTRIAL PLANET FORMATION; MAIN-SEQUENCE STARS;
CIRCUMSTELLAR DISK; KUIPER-BELT; SPACE-TELESCOPE; HD 207129; HOT DUST;
COLLISIONAL EVOLUTION; SOLAR NEIGHBORHOOD
AB We present far-infrared and submillimeter images of the eta Crv debris disk system obtained with Herschel and SCUBA-2, as well as Hubble Space Telescope visible and near-infrared coronagraphic images. In the 70 mu m Herschel image, we clearly separate the thermal emission from the warm and cold belts in the system, find no evidence for a putative dust population located between them, and precisely determine the geometry of the outer belt. We also find marginal evidence for azimuthal asymmetries and a global offset of the outer debris ring relative to the central star. Finally, we place stringent upper limits on the scattered light surface brightness of the outer ring. Using radiative transfer modeling, we find that it is impossible to account for all observed properties of the system under the assumption that both rings contain dust populations with the same properties. While the outer belt is in reasonable agreement with the expectations of steady-state collisional cascade models, albeit with a minimum grain size that is four times larger than the blow-out size, the inner belt appears to contain copious amounts of small dust grains, possibly below the blow-out size. This suggests that the inner belt cannot result from a simple transport of grains from the outer belt and rather supports a more violent phenomenon as its origin. We also find that the emission from the inner belt has not declined over three decades, a much longer timescale than its dynamical timescale, which indicates that the belt is efficiently replenished.
C1 [Duchene, G.; Arriaga, P.; Kalas, P.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Wyatt, M.; Kennedy, G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Sibthorpe, B.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands.
[Lisse, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Holland, W.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Wisniewski, J.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Clampin, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pinte, C.] France UMI 3386, CNRS INSU, UMI FCA, Paris, France.
[Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Booth, M.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile.
[Horner, J.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Horner, J.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia.
[Matthews, B.] Natl Res Council Canada Herzberg Astron & Astroph, Victoria, BC V9E 2E7, Canada.
[Greaves, J.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
RP Duchene, G (reprint author), UJF Grenoble 1, CNRS, INSU, Inst Planetol & Astrophys IPAG,UMR 5274, F-38041 Grenoble, France.
RI Lisse, Carey/B-7772-2016
OI Lisse, Carey/0000-0002-9548-1526
FU NASA [1353184, NNX11AD21G]; ANR [ANR-07-BLAN-0221,
ANR-2010-JCJC-0504-01, ANR-2010-JCJC-0501-01]; European Commission's
7th Framework Program [PERG06-GA-2009-256513]; European Union
through ERC [279973]; NSF [AST-0909188]; JPL/NASA [NMO711043]; NSERC
Discovery Accelerator Supplement
FX We are grateful to Tushar Mittal, Christine Chen, and Karl Stapelfeldt
for discussions regarding various aspects of the data analyzed here, and
to Angelo Ricarte and Noel Moldvai for their contribution to the
modified blackbody model used in this work. We thank the DEBRIS team for
many and varied fruitful discussions throughout the duration of this
project. In particular, we are grateful to Paul Harvey for his review of
a draft of this manuscript. Comments from an anonymous referee also
helped improved this manuscript. This work was supported in part by NASA
through a contract (No. 1353184, PI: H. M. Butner) issued by the Jet
Propulsion Laboratory, California Institute of Technology under contract
with NASA. We acknowledge the Service Commun de Calcul Intensif de
l'Observatoire de Grenoble (SCCI) for computations on the super-computer
funded by ANR (contracts ANR-07-BLAN-0221, ANR-2010-JCJC-0504-01 and
ANR-2010-JCJC-0501-01) and the European Commission's 7th
Framework Program (contract PERG06-GA-2009-256513). M.W. and G.K. are
grateful for support from the European Union through ERC grant number
279973. C.L. acknowledges support from grants NASA NNX11AB21G and NSF
AAG-NNX09AU31G in working on this project. P.K. acknowledges support
from NASA NNX11AD21G, NSF AST-0909188, and JPL/NASA award NMO711043.
M.B. acknowledges support from an NSERC Discovery Accelerator
Supplement. Data presented in this paper were obtained with Herschel, an
ESA space observatory with science instruments provided by European-led
Principal Investigator consortia and with important participation from
NASA. Additional data presented in this work were obtained at the JCMT,
which is operated by the Joint Astronomy Centre on behalf of the Science
and Technology Facilities Council of the UK, the Netherlands
Organisation for Scientific Research and the National Research Council
of Canada. Additional funds for the construction of SCUBA-2 were
provided by the Canada Foundation for Innovation. 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 research has
made use of the SIMBAD database, operated at CDS, Strasbourg, France,
and of the NASA/IPAC Infrared Science Archive, which is operated by the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
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SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
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DI 10.1088/0004-637X/784/2/148
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400063
ER
PT J
AU Hamaguchi, K
Corcoran, MF
Russell, CMP
Pollock, AMT
Gull, TR
Teodoro, M
Madura, TI
Damineli, A
Pittard, JM
AF Hamaguchi, Kenji
Corcoran, Michael F.
Russell, Christopher M. P.
Pollock, A. M. T.
Gull, Theodore R.
Teodoro, Mairan
Madura, Thomas I.
Damineli, Augusto
Pittard, Julian M.
TI X-RAY EMISSION FROM ETA CARINAE NEAR PERIASTRON IN 2009. I. A TWO-STATE
SOLUTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; stars: early-type; stars: individual (Eta Carinae);
stars: winds; outflows X-rays: stars
ID BINARY WR 140; COLLIDING WINDS; EVENT; COMPANION; VARIABILITY;
LAMBDA-4686; COLLISION; MINIMUM; STARS
AB X-ray emission from the supermassive binary system. Car declines sharply around periastron. This X-ray minimum has two distinct phases-the lowest flux phase in the first similar to 3 weeks and a brighter phase thereafter. In 2009, the Chandra X-ray Observatory monitored the first phase five times and found the lowest observed flux at similar to 1.9 x 10(-12) erg cm(-2) s(-1) (3-8 keV). The spectral shape changed such that the hard band above similar to 4 keV dropped quickly at the beginning and the soft band flux gradually decreased to its lowest observed value in similar to 2 weeks. The hard band spectrum had begun to recover by that time. This spectral variation suggests that the shocked gas producing the hottest X-ray gas near the apex of the wind-wind collision (WWC) is blocked behind the dense inner wind of the primary star, which later occults slightly cooler gas downstream. Shocked gas previously produced by the system at earlier orbital phases is suggested to produce the faint residual X-ray emission seen when the emission near the apex is completely blocked by the primary wind. The brighter phase is probably caused by the re-appearance of the WWC plasma, whose emissivity significantly declined during the occultation. We interpret this to mean that the X-ray minimum is produced by a hybrid mechanism of an occultation and a decline in the emissivity of the WWC shock. We constrain timings of superior conjunction and periastron based on these results.
C1 [Hamaguchi, Kenji; Corcoran, Michael F.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
[Hamaguchi, Kenji; Corcoran, Michael F.] NASA, Xray Astrophys Lab, GSFC, Greenbelt, MD 20771 USA.
[Hamaguchi, Kenji] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Corcoran, Michael F.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Russell, Christopher M. P.] Hokkai Gakuen Univ, Fac Engn, Toyohira Ku, Sapporo, Hokkaido 0628605, Japan.
[Pollock, A. M. T.] European Space Agcy, E-28691 Madrid, Spain.
[Gull, Theodore R.; Teodoro, Mairan; Madura, Thomas I.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Damineli, Augusto] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508900 Sao Paulo, Brazil.
[Pittard, Julian M.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
RP Hamaguchi, K (reprint author), NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
EM Kenji.Hamaguchi@nasa.gov
RI Damineli, Augusto/P-8829-2016;
OI Damineli, Augusto/0000-0002-7978-2994; Pittard,
Julian/0000-0003-2244-5070
FU NASA's Astrobiology Institute [RTOP 344-53-51]
FX This work was performed while K. H. was supported by the NASA's
Astrobiology Institute (RTOP 344-53-51) to the Goddard Center for
Astrobiology (PI: Michael J. Mumma). 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. We
appreciate the Chandra operation scientist Scott J. Wolk for important
advice on enhancing efficiency of the Chandra observations and useful
comments on the paper draft by David B. Henley and Kris Davidson.
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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 APR 1
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AR 125
DI 10.1088/0004-637X/784/2/125
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400040
ER
PT J
AU Hardegree-Ullman, EE
Gudipati, MS
Boogert, ACA
Lignell, H
Allamandola, LJ
Stapelfeldt, KR
Werner, M
AF Hardegree-Ullman, E. E.
Gudipati, M. S.
Boogert, A. C. A.
Lignell, H.
Allamandola, L. J.
Stapelfeldt, K. R.
Werner, M.
TI LABORATORY DETERMINATION OF THE INFRARED BAND STRENGTHS OF PYRENE FROZEN
IN WATER ICE: IMPLICATIONS FOR THE COMPOSITION OF INTERSTELLAR ICES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; infrared: ISM; ISM: abundances; methods: laboratory:
molecular; stars: protostars
ID POLYCYCLIC AROMATIC-HYDROCARBONS; YOUNG STELLAR OBJECTS; 3 MICRON
SPECTRA; SPECTROSCOPIC DATABASE; ABSORPTION FEATURES; MONOCEROS
R2/IRS-3; FACILE GENERATION; RADICAL CATIONS; AMINO-ACIDS; SOLID H2O
AB Broad infrared emission features (e.g., at 3.3, 6.2, 7.7, 8.6, and 11.3 mu m) from the gas phase interstellar medium have long been attributed to polycyclic aromatic hydrocarbons (PAHs). A significant portion (10%-20%) of the Milky Way's carbon reservoir is locked in PAH molecules, which makes their characterization integral to our understanding of astrochemistry. In molecular clouds and the dense envelopes and disks of young stellar objects (YSOs), PAHs are expected to be frozen in the icy mantles of dust grains where they should reveal themselves through infrared absorption. To facilitate the search for frozen interstellar PAHs, laboratory experiments were conducted to determine the positions and strengths of the bands of pyrene mixed with H2O and D2O ices. The D2O mixtures are used tomeasure pyrene bands that aremasked by the strong bands of H2O, leading to the first laboratory determination of the band strength for the CH stretching mode of pyrene in water ice near 3.25 mu m. Our infrared band strengths were normalized to experimentally determined ultraviolet band strengths, and we find that they are generally similar to 50% larger than those reported by Bouwman et al. based on theoretical strengths. These improved band strengths were used to reexamine YSO spectra published by Boogert et al. to estimate the contribution of frozen PAHs to absorption in the 5-8 mu m spectral region, taking into account the strength of the 3.25 mu m CH stretching mode. It is found that frozen neutral PAHs contain 5%-9% of the cosmic carbon budget and account for 2%-9% of the unidentified absorption in the 5-8 mu m region.
C1 [Hardegree-Ullman, E. E.] Rensselaer Polytech Inst, New York Ctr Astrobiol, Troy, NY 12180 USA.
[Hardegree-Ullman, E. E.] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA.
[Hardegree-Ullman, E. E.; Boogert, A. C. A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Gudipati, M. S.; Werner, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gudipati, M. S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
[Boogert, A. C. A.] NASA Ames Res Ctr, SOFIA Sci Ctr, USRA, Moffett Field, CA 94035 USA.
[Lignell, H.] Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA.
[Lignell, H.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
[Allamandola, L. J.] NASA Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Stapelfeldt, K. R.] NASA Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
RP Hardegree-Ullman, EE (reprint author), Rensselaer Polytech Inst, New York Ctr Astrobiol, 110 8th St, Troy, NY 12180 USA.
EM hardee@rpi.edu; gudipati@jpl.nasa.gov
RI Gudipati, Murthy/F-7575-2011
FU NASA Astrobiology Institute to Rensselaer Polytechnic Institute
[NNA09DA80A]; Jet Propulsion Laboratory's DRDF and R&TD funding for
infrastructure of the "Ice Spectroscopy Laboratory"; Spitzer Space
Telescope; Finnish Cultural Foundation; IPAC Visiting Graduate Student
Fellowship
FX This research was carried out at the Jet Propulsion Laboratory and IPAC,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. Support for this research was
provided in part by funding from the NASA Astrobiology Institute to
Rensselaer Polytechnic Institute (award NNA09DA80A). The experimental
part of this work was enabled through partial funding from the Jet
Propulsion Laboratory's DRDF and R&TD funding for infrastructure of the
"Ice Spectroscopy Laboratory" and was carried out by H.L. and M. S. G.,
supported by an astrophysics laboratory research award funded by the
Spitzer Space Telescope. H.L. also acknowledges the Finnish Cultural
Foundation for financial support. We thank Dr. Irene Li Barnett and Dr.
Antti Lignell, who were involved in building the experimental setup used
and initial training of H.L. Data analysis was carried out by E.H-U. at
the California Institute of Technology (supervised by A.B. and M.S.G.),
funded by an IPAC Visiting Graduate Student Fellowship.
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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 APR 1
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DI 10.1088/0004-637X/784/2/172
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400087
ER
PT J
AU Lionello, R
Velli, M
Downs, C
Linker, JA
Mikic, Z
Verdini, A
AF Lionello, Roberto
Velli, Marco
Downs, Cooper
Linker, Jon A.
Mikic, Zoran
Verdini, Andrea
TI VALIDATING A TIME-DEPENDENT TURBULENCE-DRIVEN MODEL OF THE SOLAR WIND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); solar wind; turbulence; waves
ID ALFVEN WAVES; MHD TURBULENCE; CORONAL HOLES; MAGNETOHYDRODYNAMIC
TURBULENCE; TRANSITION REGION; STELLAR CORONAE; ENERGY-BALANCE;
ACCELERATION; TRANSPORT; FLOW
AB Although the mechanisms responsible for heating the Sun's corona and accelerating the solar wind are still being actively investigated, it is largely accepted that photospheric motions provide the energy source and that the magnetic field must play a key role in the process. Verdini et al. presented a model for heating and accelerating the solar wind based on the turbulent dissipation of Alfven waves. We first use a time-dependent model of the solar wind to reproduce one of Verdini et al.'s solutions; then, we extend its application to the case where the energy equation includes thermal conduction and radiation losses, and the upper chromosphere is part of the computational domain. Using this model, we explore the parameter space and describe the characteristics of a fast solar wind solution. We discuss how this formulation may be applied to a three-dimensional MHD model of the corona and solar wind.
C1 [Lionello, Roberto; Downs, Cooper; Linker, Jon A.; Mikic, Zoran] Predict Sci Inc, San Diego, CA 92121 USA.
[Velli, Marco] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Verdini, Andrea] Observ Royal Belgique, B-1180 Brussels, Belgium.
RP Lionello, R (reprint author), Predict Sci Inc, 9990 Mesa Rim Rd,Suite 170, San Diego, CA 92121 USA.
EM lionel@predsci.com; mvelli@mail.jpl.nasa.gov; cdowns@predsci.com;
linker@predsci.com; mikic@predsci.com; verdini@oma.be
FU NASA's LWS TR&T and HTP programs; Center for Integrated Space Weather
Modeling; NASA Solar Probe Plus Observatory Scientist contract; Texas
Advanced Computing Center (TACC) in Austin; NASA Advanced Supercomputing
Division (NAS) at Ames Research Center
FX Work carried out at PSI was supported by NASA's LWS TR&T and HTP
programs, and the Center for Integrated Space Weather Modeling (an NSF
Science and Technology Center). This work was carried out in part by the
Jet Propulsion Laboratory, California Institute of Technology under a
contract with NASA. M. V. was supported by the NASA Solar Probe Plus
Observatory Scientist contract. Computational resources were provided by
the NSF supported Texas Advanced Computing Center (TACC) in Austin and
the NASA Advanced Supercomputing Division (NAS) at Ames Research Center.
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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 APR 1
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SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400035
ER
PT J
AU Mackay, DH
DeVore, CR
Antiochos, SK
AF Mackay, Duncan H.
DeVore, C. Richard
Antiochos, Spiro K.
TI GLOBAL-SCALE CONSEQUENCES OF MAGNETIC-HELICITY INJECTION AND
CONDENSATION ON THE SUN
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; Sun: activity; Sun: corona
ID DRIVEN VORTEX FLOWS; SOLAR CORONA; HEMISPHERIC PATTERN; FILAMENT
CHANNELS; FLUX TRANSPORT; FINE-STRUCTURE; FIELDS; PROMINENCES;
CHIRALITY; EVOLUTION
AB In the recent paper of Antiochos, a new concept for the injection of magnetic helicity into the solar corona by small-scale convective motions and its condensation onto polarity inversion lines (PILs) was developed. We investigate this concept through global simulations of the Sun's photospheric and coronal magnetic fields, and compare the results with the hemispheric pattern of solar filaments. Assuming that the vorticity of the cells is predominantly counterclockwise/clockwise in the northern/southern hemisphere, the convective motions inject negative/positive helicity into each hemisphere. The simulations show that: (1) on a north-south oriented PIL, both differential rotation and convective motions inject the same sign of helicity, which matches that required to reproduce the hemispheric pattern of filaments. (2) On a high-latitude east-west oriented polar crown or subpolar crown PIL, the vorticity of the cells has to be approximately 2-3 times greater than the local differential-rotation gradient in order to overcome the incorrect sign of helicity injection from differential rotation. (3) In the declining phase of the cycle, as a bipole interacts with the polar field, in some cases, helicity condensation can reverse the effect of differential rotation along the east-west lead arm but not in all cases. The results show that this newly developed concept of magnetic helicity injection and condensation, in conjunction with the mechanisms used in Yeates et al., is a viable explanation for the hemispheric pattern of filaments. Future observational studies should focus on examining the vorticity component within convective motions to determine both its magnitude and latitudinal variation relative to the differential-rotation gradient on the Sun.
C1 [Mackay, Duncan H.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
[DeVore, C. Richard] Naval Res Lab, Washington, DC 20375 USA.
[DeVore, C. Richard; Antiochos, Spiro K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Mackay, DH (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
EM dhm@st-and.ac.uk
RI DeVore, C/A-6067-2015; Antiochos, Spiro/D-4668-2012
OI DeVore, C/0000-0002-4668-591X; Antiochos, Spiro/0000-0003-0176-4312
FU STFC; Leverhulme Trust; European Commission [263340]; NASA TR&T and SRT
programs
FX D.H.M. would like to thank STFC, the Leverhulme Trust, and the European
Commission's Seventh Framework Programme (FP7/2007-2013) under grant
agreement SWIFF (project 263340, http://www.swiff.eu) for their
financial support. C.R.D. and S.K.A. wish to acknowledge the NASA TR&T
and SR&T programs for supporting their contributions to the work. All of
us thank Judy Karpen for lending her artistic expertise in creating the
figures used in the Appendix and for helpful comments on the manuscript.
We also appreciate Anthony Yeates' alerting us to the observations of
J.A. Bonet and collaborators. D.H.M. and C.R.D. participated in a team
investigation of solar prominences at the International Space Science
Institute, where this collaboration was conceived and initiated. We are
grateful to ISSI for hosting us, to Nicolas Labrosse for leading the
team, and to Zoran Mikic and the rest of the group for stimulating
discussions.
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SN 0004-637X
EI 1538-4357
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400079
ER
PT J
AU Mainzer, A
Bauer, J
Grav, T
Masiero, J
Cutri, RM
Wright, E
Nugent, CR
Stevenson, R
Clyne, E
Cukrov, G
Masci, F
AF Mainzer, A.
Bauer, J.
Grav, T.
Masiero, J.
Cutri, R. M.
Wright, E.
Nugent, C. R.
Stevenson, R.
Clyne, E.
Cukrov, G.
Masci, F.
TI THE POPULATION OF TINY NEAR-EARTH OBJECTS OBSERVED BY NEOWISE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atlases; catalogs; infrared: general; minor planets; asteroids: general;
surveys
ID THERMAL-MODEL CALIBRATION; INFRARED-SURVEY-EXPLORER; WISE/NEOWISE
OBSERVATIONS; PHASE CURVES; ASTEROIDS; PHOTOMETRY; SYSTEM
AB Only a very small fraction of the asteroid population at size scales comparable to the object that exploded over Chelyabinsk, Russia has been discovered to date, and physical properties are poorly characterized. We present previously unreported detections of 105 close approaching near-Earth objects (NEOs) by the Wide-field Infrared Survey Explorer (WISE) mission's NEOWISE project. These infrared observations constrain physical properties such as diameter and albedo for these objects, many of which are found to be smaller than 100 m. Because these objects are intrinsically faint, they were detected by WISE during very close approaches to the Earth, often at large apparent on-sky velocities. We observe a trend of increasing albedo with decreasing size, but as this sample of NEOs was discovered by visible light surveys, it is likely that selection biases against finding small, dark NEOs influence this finding.
C1 [Mainzer, A.; Bauer, J.; Masiero, J.; Nugent, C. R.; Stevenson, R.; Clyne, E.; Cukrov, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, J.; Cutri, R. M.; Masci, F.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Wright, E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM amainzer@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X
FU National Aeronautics and Space Administration; Planetary Science
Division of the National Aeronautics and Space Administration
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 the Jet Propulsion Laboratory/California
Institute of Technology, funded by the Planetary Science Division of the
National Aeronautics and Space Administration. We thank our referee, Dr.
Alan Harris of Pasadena, for his helpful comments that materially
improved this manuscript. We gratefully acknowledge the extraordinary
services specific to NEOWISE contributed by the International
Astronomical Union's Minor Planet Center, operated by the
Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for
Astronomical Telegrams, operated by Harvard University. We also thank
the worldwide community of dedicated amateur and professional
astronomers devoted to minor planet follow-up observations. This
research has made use of the NASA/IPAC Infrared Science Archive, which
is operated by the California Institute of Technology, under contract
with the National Aeronautics and Space Administration.
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SN 0004-637X
EI 1538-4357
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JI Astrophys. J.
PD APR 1
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SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400025
ER
PT J
AU Nguyen, AN
Messenger, S
AF Nguyen, Ann N.
Messenger, Scott
TI RESOLVING THE STELLAR SOURCES OF ISOTOPICALLY RARE PRESOLAR SILICATE
GRAINS THROUGH Mg AND Fe ISOTOPIC ANALYSES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; novae, cataclysmic variables; nuclear reactions,
nucleosynthesis, abundances; stars: winds, outflows; supernovae: general
ID ASYMPTOTIC GIANT BRANCH; LARGE-MAGELLANIC-CLOUD; AGB STARS; MASSIVE
STARS; SOLAR-SYSTEM; SIC GRAINS; CARBONACEOUS CHONDRITE; INTERSTELLAR
GRAINS; CHEMICAL EVOLUTION; GALACTIC EVOLUTION
AB We conducted multi-element isotopic analyses of 11 presolar silicate grains from the Acfer 094 meteorite having unusual O isotopic compositions. Eight grains are O-18-rich, one is O-16-rich, and two are extremely O-17-rich. We constrained the grains' stellar sources by measuring their Si and Mg isotopic ratios, and also the Fe-54/Fe-56 and Fe-57/Fe-56 ratios for five grains. The Mg and Fe isotopic measurements were conducted after surrounding matrix grains were removed for more accurate ratios. Most of the O-18-rich silicates had anomalous Mg isotopic ratios, and their combined isotopic constraints are consistent with origins in low-mass Type II supernovae (SNe II) rather than high-metallicity stars. The isotopic ratios of the O-16-rich silicate are also consistent with an SN origin. Mixing small amounts of interior stellar material with the stellar envelope replicated all measured isotopic ratios except for Si-29/ Si-28 and Fe-54/Fe-56 in some grains. The Si-29/Si-28 ratios of all SN-derived grains are matched by doubling the Si-29 yield in the Ne- and Si-burning zones. The Fe-54/Fe-56 ratios of the grains imply elemental fractionation in the Si/S zone, or introduction of isotopically solar Fe by secondary processing. The two highly 17O-rich silicates exhibited significant Mg-25 and/or Mg-26 enrichments and their isotopic ratios are best explained by strong dilution of 1.15M(circle dot) CO nova matter. We estimate that similar to 12% and 1% of presolar silicates have SN and nova origins, respectively, similar to presolar SiC and oxides. This implies that asymptotic giant branch stars are the dominant dust producers in the galaxy.
C1 [Nguyen, Ann N.; Messenger, Scott] NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA.
[Nguyen, Ann N.] NASA, Lyndon B Johnson Space Ctr, Jacobs, Houston, TX 77058 USA.
RP Nguyen, AN (reprint author), NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA.
EM lan-anh.n.nguyen@nasa.gov
FU NASA Cosmochemistry [12-COS12-0058]
FX We thank M. Ito for assistance with Mg isotopic measurements and Z.
Rahman for FIB preparation of the samples. We are grateful to F.
Gyngard, S. Woosley, and A. Heger for providing stellar model results.
This manuscript was improved by comments from an anonymous reviewer.
This work was supported by NASA Cosmochemistry grant 12-COS12-0058.
NR 84
TC 5
Z9 5
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 APR 1
PY 2014
VL 784
IS 2
AR 149
DI 10.1088/0004-637X/784/2/149
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400064
ER
PT J
AU Peacock, MB
Zepf, SE
Maccarone, TJ
Kundu, A
Gonzalez, AH
Lehmer, BD
Maraston, C
AF Peacock, Mark B.
Zepf, Stephen E.
Maccarone, Thomas J.
Kundu, Arunav
Gonzalez, Anthony H.
Lehmer, Bret D.
Maraston, Claudia
TI EVIDENCE FOR A CONSTANT INITIAL MASS FUNCTION IN EARLY-TYPE GALAXIES
BASED ON THEIR X-RAY BINARY POPULATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: stellar content;
stars: luminosity function; mass function; X-rays: binaries
ID CHANDRA MONITORING OBSERVATIONS; GLOBULAR-CLUSTER CONNECTION;
HUBBLE-SPACE-TELESCOPE; SURFACE BRIGHTNESS FLUCTUATIONS; INFRARED
FUNDAMENTAL PLANE; ELLIPTIC GALAXIES; STELLAR POPULATIONS; DEEP CHANDRA;
SYSTEMATIC VARIATION; LUMINOSITY FUNCTIONS
AB A number of recent studies have proposed that the stellar initial mass function (IMF) of early type galaxies varies systematically as a function of galaxy mass, with higher mass galaxies having bottom-heavy IMFs. These bottom-heavy IMFs have more low-mass stars relative to the number of high mass stars, and therefore naturally result in proportionally fewer neutron stars (NSs) and black holes (BHs). In this paper, we specifically predict the variation in the number of BHs and NSs based on the power-law IMF variation required to reproduce the observed mass-to-light ratio trends with galaxy mass. We then test whether such variations are observed by studying the field low-mass X-ray binary (LMXB) populations of nearby early-type galaxies. In these binaries, an NS or BH accretes matter from a low-mass donor star. Their number is therefore expected to scale with the number of BHs and NSs present in a galaxy. We find that the number of LMXBs per K-band light is similar among the galaxies in our sample. These data therefore demonstrate the uniformity of the slope of the IMF from massive stars down to those now dominating the K-band light and are consistent with an invariant IMF. Our results are inconsistent with an IMF which varies from a Kroupa/Chabrier like IMF for low-mass galaxies to a steep power-law IMF (with slope x = 2.8) for high mass galaxies. We discuss how these observations constrain the possible forms of the IMF variations and how future Chandra observations can enable sharper tests of the IMF.
C1 [Peacock, Mark B.; Zepf, Stephen E.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Maccarone, Thomas J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
[Kundu, Arunav] Eureka Sci Inc, Oakland, CA 100 USA.
[Kundu, Arunav] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Lehmer, Bret D.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Lehmer, Bret D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Maraston, Claudia] Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
RP Peacock, MB (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
EM mpeacock@msu.edu
FU NASA through ADAP [NNX11AG12G]; Chandra [AR4-15007X]; NASA through
Chandra [GO0-11111A, AR1-12009X]
FX M.B.P. and S.E.Z. acknowledge support from NASA through the ADAP grant
NNX11AG12G and through the Chandra award AR4-15007X. A.K. acknowledges
support for this work provided by NASA through Chandra awards GO0-11111A
and AR1-12009X.
NR 88
TC 16
Z9 16
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2014
VL 784
IS 2
AR 162
DI 10.1088/0004-637X/784/2/162
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400077
ER
PT J
AU Regnier, S
Alexander, CE
Walsh, RW
Winebarger, AR
Cirtain, J
Golub, L
Korreck, KE
Mitchell, N
Platt, S
Weber, M
De Pontieu, B
Title, A
Kobayashi, K
Kuzin, S
DeForest, CE
AF Regnier, S.
Alexander, C. E.
Walsh, R. W.
Winebarger, A. R.
Cirtain, J.
Golub, L.
Korreck, K. E.
Mitchell, N.
Platt, S.
Weber, M.
De Pontieu, B.
Title, A.
Kobayashi, K.
Kuzin, S.
DeForest, C. E.
TI SPARKLING EXTREME-ULTRAVIOLET BRIGHT DOTS OBSERVED WITH Hi-C
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: corona; Sun: magnetic fields; Sun: UV radiation
ID DYNAMICS-OBSERVATORY SDO; SOLAR MAGNETIC ELEMENTS; CORONA; REGIONS;
DIAGNOSTICS; NANOFLARES; RESOLUTION; TELESCOPE; EVENTS; PLASMA
AB Observing the Sun at high time and spatial scales is a step toward understanding the finest and fundamental scales of heating events in the solar corona. The high-resolution coronal (Hi-C) instrument has provided the highest spatial and temporal resolution images of the solar corona in the EUV wavelength range to date. Hi-C observed an active region on 2012 July 11 that exhibits several interesting features in the EUV line at 193 angstrom. One of them is the existence of short, small brightenings "sparkling" at the edge of the active region; we call these EUV bright dots (EBDs). Individual EBDs have a characteristic duration of 25 s with a characteristic length of 680 km. These brightenings are not fully resolved by the SDO/AIA instrument at the same wavelength; however, they can be identified with respect to the Hi-C location of the EBDs. In addition, EBDs are seen in other chromospheric/coronal channels of SDO/AIA, which suggests a temperature between 0.5 and 1.5 MK. Based on their frequency in the Hi-C time series, we define four different categories of EBDs: single peak, double peak, long duration, and bursty. Based on a potential field extrapolation from an SDO/HMI magnetogram, the EBDs appear at the footpoints of large-scale, trans-equatorial coronal loops. The Hi-C observations provide the first evidence of small-scale EUV heating events at the base of these coronal loops, which have a free magnetic energy of the order of 10(26) erg.
C1 [Regnier, S.; Alexander, C. E.; Walsh, R. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Winebarger, A. R.; Cirtain, J.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Golub, L.; Korreck, K. E.; Weber, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mitchell, N.; Platt, S.] Univ Cent Lancashire, Sch Comp Engn & Phys Sci, Preston PR1 2HE, Lancs, England.
[De Pontieu, B.; Title, A.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Kobayashi, K.] Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA.
[Kuzin, S.] Russian Acad Sci, PN Lebedev Phys Inst, Moscow 119991, Russia.
[DeForest, C. E.] Southwest Res Inst, Boulder, CO 80302 USA.
RP Regnier, S (reprint author), Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
RI Regnier, Stephane/H-9107-2012; Kuzin, Sergey/M-3435-2015; Regnier,
Stephane/K-2423-2015; Platt, Simon/C-6048-2008
OI Regnier, Stephane/0000-0001-8954-4183; Regnier,
Stephane/0000-0001-8954-4183; Platt, Simon/0000-0003-4431-8814
NR 32
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
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2014
VL 784
IS 2
AR 134
DI 10.1088/0004-637X/784/2/134
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400049
ER
PT J
AU Scully, ST
Malkan, MA
Stecker, FW
AF Scully, Sean T.
Malkan, Matthew A.
Stecker, Floyd W.
TI AN EMPIRICAL DETERMINATION OF THE INTERGALACTIC BACKGROUND LIGHT USING
NEAR-INFRARED DEEP GALAXY SURVEY DATA OUT TO 5 mu m AND THE GAMMA-RAY
OPACITY OF THE UNIVERSE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (PKS 1424+240); diffuse radiation; gamma
rays: general
ID LUMINOSITY FUNCTION; OPTICAL DEPTH; PKS 1424+240; LOWER-LIMIT; K-BAND;
TO 4; EVOLUTION; REDSHIFT; SPECTRA; BLAZARS
AB We extend our previous model-independent determination of the intergalactic background light, based purely on galaxy survey data, out to a wavelength of 5 mu m. Our approach enables us to constrain the range of photon densities, based on the uncertainties from observationally determined luminosity densities and colors. We further determine a 68% confidence upper and lower limit on the opacity of the universe to gamma-rays up to energies of 1.6/(1 + z) TeV. A comparison of our lower limit redshift-dependent opacity curves to the opacity limits derived from the results of both ground-based air Cerenkov telescope and Fermi-LAT observations of PKS 1424+240 allows us to place a new upper limit on the redshift of this source, independent of IBL modeling.
C1 [Scully, Sean T.] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA.
[Malkan, Matthew A.; Stecker, Floyd W.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Stecker, Floyd W.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Scully, ST (reprint author), James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA.
EM Floyd.W.Stecker@nasa.gov
NR 43
TC 10
Z9 10
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2014
VL 784
IS 2
AR 138
DI 10.1088/0004-637X/784/2/138
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400053
ER
PT J
AU Swain, MR
Line, MR
Deroo, P
AF Swain, Mark R.
Line, Michael R.
Deroo, Pieter
TI ON THE DETECTION OF MOLECULES IN THE ATMOSPHERE OF HD 189733b USING HST
NICMOS TRANSMISSION SPECTROSCOPY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; planetary systems; planets and satellites:
atmospheres; planets and satellites: individual (HD 189733b); radiative
transfer
ID HUBBLE-SPACE-TELESCOPE; KECK INTERFEROMETER; EXTRASOLAR PLANET;
SUPER-EARTHS; SPECTRUM; WATER; RETRIEVAL; HD189733B; WASP-12B; 209458B
AB The Hubble Space Telescope/NICMOS transmission spectrum measurements of HD 189733b that suggest the detection of methane (CH4) in an exoplanet atmosphere have been a source of significant controversy. With what is probably the best analyzed exoplanet spectroscopy data set to date, different teams, using different methods, have claimed evidence both contradicting and supporting the original findings. Here, we report results from a uniform spectral retrieval analysis of the three independent published spectra together with null hypothesis testing. Based on Bayesian model comparison, we find that two of the three spectra show strong evidence (>= 3.6 sigma) for the detection of molecular features mainly due to water and methane while the third is consistent with a weak molecular detection at the 2.2 sigma level. We interpret the agreement in the spectral modulation established by previous authors and the atmospheric retrieval results presented here, as a confirmation of the original detection of molecular absorbers in the atmosphere of HD 189733b.
C1 [Swain, Mark R.; Deroo, Pieter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Line, Michael R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
RP Swain, MR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Mark.R.Swain@jpl.nasa.gov
NR 44
TC 21
Z9 21
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2014
VL 784
IS 2
AR 133
DI 10.1088/0004-637X/784/2/133
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG6HJ
UT WOS:000335519400048
ER
PT J
AU Acikmese, B
Mandic, M
Speyer, JL
AF Acikmese, Behcet
Mandic, Milan
Speyer, Jason L.
TI Decentralized observers with consensus filters for distributed
discrete-time linear systems
SO AUTOMATICA
LA English
DT Article
DE Observers; Distributed systems; Graph theory; Linear matrix inequalities
ID MULTIAGENT SYSTEMS; COMMUNICATION; ESTIMATORS; TOPOLOGIES; NETWORKS;
GRAPHS; AGENTS
AB This paper presents a decentralized observer with a consensus filter for the state observation of discrete-time linear distributed systems. Each agent in the distributed system has an observer with a model of the plant that utilizes the set of locally available measurements, which may not make the full plant state detectable. This lack of detectability is overcome by utilizing a consensus filter that blends the state estimate of each agent with its neighbors' estimates. It is proven that the state estimates of the proposed observer exponentially converge to the actual plant states under arbitrarily changing, but connected, communication and pseudo-connected sensing graph topologies. Except these connectivity properties, full knowledge of the sensing and communication graphs is not needed at the design time. As a byproduct, we obtained a result on the location of eigenvalues, i.e., the spectrum, of the Laplacian for a family of graphs with self-loops. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Acikmese, Behcet] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA.
[Mandic, Milan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Speyer, Jason L.] Univ Calif Los Angeles, Mech & Aerosp Engn Dept, Los Angeles, CA 90095 USA.
[Speyer, Jason L.] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA.
RP Acikmese, B (reprint author), Univ Texas Austin, Dept Aerosp Engn & Engn Mech, 210 E 24th St, Austin, TX 78712 USA.
EM behcet@austin.utexas.edu; Milan.Mandic@jpl.nasa.gov;
speyer@seas.ucla.edu
NR 34
TC 8
Z9 8
U1 2
U2 20
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0005-1098
EI 1873-2836
J9 AUTOMATICA
JI Automatica
PD APR
PY 2014
VL 50
IS 4
BP 1037
EP 1052
DI 10.1016/j.automatica.2014.02.008
PG 16
WC Automation & Control Systems; Engineering, Electrical & Electronic
SC Automation & Control Systems; Engineering
GA AG7WA
UT WOS:000335628300004
ER
PT J
AU Friedman, BH
Stephens, CL
Thayer, JF
AF Friedman, Bruce H.
Stephens, Chad L.
Thayer, Julian F.
TI Redundancy analysis of autonomic and self-reported, responses to induced
emotions
SO BIOLOGICAL PSYCHOLOGY
LA English
DT Article
DE Emotion concordance; Emotion synchrony; Autonomic nervous system;
Multivariate analysis; Redundancy analysis
ID TORONTO-ALEXITHYMIA-SCALE; CANONICAL CORRELATION; BASIC EMOTIONS;
NATURAL KINDS; VAGAL TONE; MULTIVARIATE; SPECIFICITY; IMAGERY;
DISCRIMINANT; PERSPECTIVE
AB The issue of concordance among the elements of emotional states has been prominent in the literature since Lang (1968) explored the topic in relation to therapy for anxiety. Since that time, a consensus has emerged that concordance among these components is relatively low. To address this issue, redundancy analysis, a technique for examining directional relationships between two sets of multivariate data, was applied to data from a previously published study (Stephens, Christie,& Friedman, 2010). Subjects in this study listened to emotion-inducing music and viewed affective films while a montage of autonomic variables, as well as self-reported affective responses, were recorded. Results indicated that approximately 27-28% of the variance in self-reported affect could be explained by autonomic variables, and vice-versa. When all of the constraints of this emotion research paradigm are considered, these levels of explained variance indicate substantial coherence between feelings and physiology during the emotion inductions. These results are considered vis-a-vis the low levels of coherence that have often been reported in the literature. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Friedman, Bruce H.] Virginia Polytech Inst & State Univ, Dept Psychol 0436, Blacksburg, VA 24061 USA.
[Stephens, Chad L.] Virginia Polytech Inst & State Univ, Blacksburg, VA 24061 USA.
[Stephens, Chad L.] NASA, Langley Res Ctr, Hampton, VA USA.
[Thayer, Julian F.] Ohio State Univ, Dept Psychol, Columbus, OH 43210 USA.
RP Friedman, BH (reprint author), Virginia Polytech Inst & State Univ, Dept Psychol 0436, Blacksburg, VA 24061 USA.
EM bhfriedm@vt.edu
NR 86
TC 8
Z9 8
U1 19
U2 37
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0301-0511
EI 1873-6246
J9 BIOL PSYCHOL
JI Biol. Psychol.
PD APR
PY 2014
VL 98
BP 19
EP 28
DI 10.1016/j.biopsycho.2013.12.006
PG 10
WC Psychology, Biological; Behavioral Sciences; Psychology; Psychology,
Experimental
SC Psychology; Behavioral Sciences
GA AG6AE
UT WOS:000335499900003
PM 24380823
ER
PT J
AU Czabaj, MW
Ratcliffe, JG
Davidson, BD
AF Czabaj, M. W.
Ratcliffe, J. G.
Davidson, B. D.
TI Observation of intralaminar cracking in the edge crack torsion specimen
SO ENGINEERING FRACTURE MECHANICS
LA English
DT Article
DE Polymer matrix composites; Toughness testing; Delamination; Mode III;
Damage tolerance; Fracture mechanics
ID III INTERLAMINAR FRACTURE; I PLUS III; COMPOSITE-MATERIALS; ECT TEST;
MODE; TOUGHNESS; SHEAR
AB The edge crack torsion (ECT) test is evaluated to determine its suitability for measuring fracture toughness associated with the onset of mode III delamination in laminated composites. ECT specimens with preimplanted midplane inserts of different lengths are tested and examined using nondestructive and destructive techniques. Ultrasonic inspections of all tested specimens reveal that delamination growth occurs one ply interface beneath the midplane. This is confirmed by sectioning and optical microscopy, which also show that macroscopic delamination advance results from a coalescence of angled intralaminar matrix cracks that form in-between and then extend through the midplane plies. The relative orientation of these intralaminar cracks is approximately 45 with respect to the midplane, suggesting that their formation is caused by resolved principal tensile stresses arising due to the global mode III shear loading. Examination of ECT specimens tested to loads below the level corresponding to the onset of delamination growth reveals that initiation of intralaminar cracking occurs prior to or concurrently with the onset of nonlinearity in the specimen's force-displacement response. The existence of intralaminar cracking prior to delamination growth and the resulting delamination extension at an unintended interface render the ECT test, in its current form, unsuitable for characterizing the onset of mode III delamination growth. The broader implications of the mechanisms observed in this study are also discussed with respect to the current understanding of shear-driven delamination in tape-laminate composites. Published by Elsevier Ltd.
C1 [Czabaj, M. W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Ratcliffe, J. G.] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Davidson, B. D.] Syracuse Univ, Syracuse, NY 13244 USA.
RP Czabaj, MW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM michael.w.czabaj@nasa.gov
NR 32
TC 5
Z9 5
U1 1
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0013-7944
EI 1873-7315
J9 ENG FRACT MECH
JI Eng. Fract. Mech.
PD APR
PY 2014
VL 120
BP 1
EP 14
DI 10.1016/j.engfracmech.2014.03.002
PG 14
WC Mechanics
SC Mechanics
GA AG7PV
UT WOS:000335611200001
ER
PT J
AU Bue, BD
AF Bue, Brian D.
TI An Evaluation of Low-Rank Mahalanobis Metric Learning Techniques for
Hyperspectral Image Classification
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Classification; Compact Reconnaissance Imaging Spectrometer for Mars
(CRISM); dimensionality reduction; hyperspectral; low rank; Mahalanobis;
metric learning
ID ALGORITHM
AB We provide a comparative study of several state-of-the-art Mahalanobis metric learning algorithms evaluated on three well-studied, high-dimensional hyperspectral images captured by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument. We focus on the problem of low-rank Mahalanobis metric learning, where our objective is to learn an n x m projection matrix, where m << n. Low-rank metrics offer a "plug-in" enhancement to similarity-based classifiers that can reduce computation time and improve classification accuracy with fewer training samples, enabling operations in resource-constrained environments such as onboard spacecraft. Our results indicate that applying a simple shrinkage-based regularization procedure to multi-class Linear Discriminant Analysis (LDA) produces comparable or better classification accuracies than the low-rank extensions of several widely used Mahalanobismetric learning algorithms, at considerably lower computational cost.
C1 CALTECH, Jet Prop Lab, NASA, Machine Learning & Instrument Auton Grp, Pasadena, CA 91101 USA.
RP Bue, BD (reprint author), CALTECH, Jet Prop Lab, NASA, Machine Learning & Instrument Auton Grp, Pasadena, CA 91101 USA.
EM bbue@jpl.nasa.gov
NR 32
TC 5
Z9 5
U1 0
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2014
VL 7
IS 4
BP 1079
EP 1088
DI 10.1109/JSTARS.2014.2302002
PG 10
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA AG4LB
UT WOS:000335390000008
ER
PT J
AU Cardoso, AS
Chakraborty, PS
Lourenco, NE
England, TD
Saha, P
Howard, DC
Fleischhauer, DM
Warner, JH
McMorrow, D
Buchner, SP
Paki-Amouzou, P
Thrivikraman, TK
Cressler, JD
AF Cardoso, Adilson S.
Chakraborty, Partha S.
Lourenco, Nelson E.
England, Troy D.
Saha, Prabir
Howard, Duane C.
Fleischhauer, David M.
Warner, Jeffrey H.
McMorrow, Dale
Buchner, Stephen P.
Paki-Amouzou, Pauline
Thrivikraman, Tushar K.
Cressler, John D.
TI Evaluating the Effects of Single Event Transients in FET-Based
Single-Pole Double-Throw RF Switches
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE Bulk FET; low insertion loss switch; radiation; RF switch; SiGe Bi CMOS;
single event transient (SET); single-pole double-throw (SPDT); SOI
ID LOW-NOISE AMPLIFIER; 130 NM CMOS; TECHNOLOGY; MITIGATION; DEVICES
AB The impact of single event transients (SETs) on single-pole double-throw (SPDT) RF switch circuits designed in a commercially-available, 180 nm second-generation SiGe BiCMOS (IBM 7HP) technology is investigated. The intended application for these SPDT RF switches requires a 1 GHz to 20 GHz band of operation, relatively low insertion loss (< 3.0 dB at 20 GHz), and moderate isolation (> 15 dB at 20 GHz). Two-photon absorption experiment results reveal that the SPDT switches are vulnerable to SETs due to biasing effects as well as the triple-well (TW) nFETs, which are found to be more sensitive to SETs than bulk nFETs. From these results, potential implications are discussed and mitigation strategies are proposed. To verify one of the proposed mitigation techniques, SPDT switches were also designed in a 180 nm twin-well SOI CMOS (IBM 7RF-SOI) technology. A different biasing technique is implemented to help improve the SET response. The fabricated SOI SPDT switches achieve an insertion loss of < 1.04 dB at 20 GHz and > 21 dB isolation at 20 GHz. For this circuit, no transients were observed even at very high laser energies (approximate to 5 nJ).
C1 [Cardoso, Adilson S.; Chakraborty, Partha S.; Lourenco, Nelson E.; England, Troy D.; Saha, Prabir; Howard, Duane C.; Fleischhauer, David M.; Cressler, John D.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA.
[Warner, Jeffrey H.; McMorrow, Dale; Buchner, Stephen P.] Naval Res Lab, Washington, DC 20375 USA.
[Paki-Amouzou, Pauline] Def Threat Reduct Agcy, Ft Belvoir, VA 22060 USA.
[Thrivikraman, Tushar K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cardoso, AS (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA.
EM cardosoa@gatech.edu
RI Chakraborty, Partha/K-6963-2014
FU Defense Threat Reduction Agency [HDTRA1-09-C-0031]; SPAWAR; NASA-NEPP
FX This work was supported in part by the Defense Threat Reduction Agency
under HDTRA1-09-C-0031, in part by SPAWAR, and in part by NASA-NEPP.
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PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD APR
PY 2014
VL 61
IS 2
BP 756
EP 765
DI 10.1109/TNS.2014.2301448
PG 10
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA AF7YI
UT WOS:000334931100008
ER
PT J
AU Prieskorn, ZR
Hill, JE
Kaaret, PE
Black, JK
AF Prieskorn, Z. R.
Hill, J. E.
Kaaret, P. E.
Black, J. K.
TI Photoelectron Track Length Distributions Measured in a Negative Ion Time
Projection Chamber
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE Negative ion time projection chamber; nitromethane; photoelectron track
length; X-ray detectors; CH3NO2
ID GAS PROPORTIONAL COUNTER; RESOLUTION; RANGE
AB We report photoelectron track length distributions between 3 and 8 keV in gas mixtures of Ne + CO2 + CH3NO2 (260: 80: 10 Torr) and CO2 + CH3NO2 (197.5: 15 Torr). The measurements were made using a negative ion time projection chamber (NITPC) at the National Synchrotron Light Source (NSLS) at the Brookhaven National Laboratory (BNL). We report the first quantitative analysis of photoelectron track length distributions in a gas. The distribution of track lengths at a given energy is best fit by a lognormal distribution. A powerlaw distribution of the form, f(E) = a(E/E-o)(n) is found to fit the relationship between mean track length and energy. We find n = 1.20 +/- 0.07 for Ne + CO2 + CH3NO2 and n = 1.20 +/-0.09 for CO2 + CH3NO2. Understanding the distribution of photoelectron track lengths in proportional counter gases is important for optimizing the pixel size and the dimensions of the active region in electron-drift time projection chambers (TPCs) and NITPC X-ray polarimeters.
C1 [Prieskorn, Z. R.] Penn State Univ, University Pk, PA 16802 USA.
[Hill, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kaaret, P. E.] Univ Iowa, Iowa City, IA 52240 USA.
[Black, J. K.] Rock Creek Sci, Silver Spring, MD 20910 USA.
RP Prieskorn, ZR (reprint author), Penn State Univ, University Pk, PA 16802 USA.
EM prieskorn@psu.edu; joanne.e.hill@nasa.gov; Philip-kaaret@uiowa.edu;
kevin.black@nasa.gov
FU NASA Goddard Space Flight Center [NNX08AF46G]
FX This work was funded under NASA grant NNX08AF46G at the NASA Goddard
Space Flight Center. Beamline X19 A at the Brookhaven National
Laboratory National Synchrotron Light Source was utilized to make the
measurements presented in this experiment. The authors would like to
thank Syed Khalid for his help at BNL. We would also like to thank
Israel Moya, Christian Urba, Richard Koenecke and Tracy L Pluchak-Rosnak
for their expert technical contributions to the project.
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PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD APR
PY 2014
VL 61
IS 2
BP 894
EP 900
DI 10.1109/TNS.2014.2312107
PG 7
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA AF7YI
UT WOS:000334931100024
ER
PT J
AU Clements, DL
Braglia, FG
Hyde, AK
Perez-Fournon, I
Bock, J
Cava, A
Chapman, S
Conley, A
Cooray, A
Farrah, D
Solares, EAG
Marchetti, L
Marsden, G
Oliver, SJ
Roseboom, IG
Schulz, B
Smith, AJ
Vaccari, M
Vieira, J
Viero, M
Wang, L
Wardlow, J
Zemcov, M
de Zotti, G
AF Clements, D. L.
Braglia, F. G.
Hyde, A. K.
Perez-Fournon, I.
Bock, J.
Cava, A.
Chapman, S.
Conley, A.
Cooray, A.
Farrah, D.
Solares, E. A. Gonzalez
Marchetti, L.
Marsden, G.
Oliver, S. J.
Roseboom, I. G.
Schulz, B.
Smith, A. J.
Vaccari, M.
Vieira, J.
Viero, M.
Wang, L.
Wardlow, J.
Zemcov, M.
de Zotti, G.
TI Herschel Multitiered Extragalactic Survey: clusters of dusty galaxies
uncovered by Herschel and Planck
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: high redshift; galaxies: starburst; submillimetre: galaxies
ID WIDE-FIELD SURVEY; DEEP SUBMILLIMETER SURVEY; IN-FLIGHT PERFORMANCE;
IRAC SHALLOW SURVEY; SIMILAR-TO 1; STAR-FORMATION; PHOTOMETRIC
REDSHIFTS; INFRARED GALAXIES; SPIRE INSTRUMENT; SPACE-TELESCOPE
AB The potential for Planck to detect clusters of dusty, star-forming galaxies at z > 1 is tested by examining the Herschel-SPIRE images of Planck Early Release Compact Source Catalog sources lying in fields observed by the Herschel Multitiered Extragalactic Survey. Of the 16 Planck sources that lie in the similar to 90 sq. deg. examined, we find that 12 are associated with single bright Herschel sources. The remaining four are associated with overdensities of Herschel sources, making them candidate clusters of dusty, star-forming galaxies. We use complementary optical/near-IR data for these 'clumps' to test this idea, and find evidence for the presence of galaxy clusters in all four cases. We use photometric redshifts and red sequence galaxies to estimate the redshifts of these clusters, finding that they range from 0.8 to 2.3. These redshifts imply that the Herschel sources in these clusters, which contribute to the detected Planck flux, are forming stars very rapidly, with typical total cluster star formation rates > 1000 M-circle dot yr(-1). The high-redshift clusters discovered in these observations are used to constrain the epoch of cluster galaxy formation, finding that the galaxies in our clusters are 1-1.5 Gyr old at z similar to 1-2. Prospects for the discovery of further clusters of dusty galaxies are discussed, using not only all sky Planck surveys, but also deeper, smaller area, Herschel surveys.
C1 [Clements, D. L.; Braglia, F. G.; Hyde, A. K.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Perez-Fournon, I.] IAC, E-38200 Tenerife, Spain.
[Perez-Fournon, I.] ULL, Dept Astrofis, E-38205 Tenerife, Spain.
[Bock, J.; Cooray, A.; Schulz, B.; Vieira, J.; Viero, M.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA.
[Bock, J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cava, A.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain.
[Cava, A.] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland.
[Chapman, S.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada.
[Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA.
[Cooray, A.; Wardlow, J.] 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.
[Marchetti, L.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Marchetti, L.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy.
[Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Astron Ctr, Brighton BN1 9QH, E Sussex, England.
[Roseboom, I. G.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Schulz, B.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa.
[de Zotti, G.] INAF OAPd, I-35122 Padua, Italy.
[de Zotti, G.] SISSA, I-34136 Trieste, Italy.
RP Clements, DL (reprint author), Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England.
EM d.clements@imperial.ac.uk
RI Wardlow, Julie/C-9903-2015; Vaccari, Mattia/R-3431-2016; Cava,
Antonio/C-5274-2017;
OI Wardlow, Julie/0000-0003-2376-8971; Vaccari, Mattia/0000-0002-6748-0577;
Cava, Antonio/0000-0002-4821-1275; De Zotti,
Gianfranco/0000-0003-2868-2595; Marchetti, Lucia/0000-0003-3948-7621
FU CSA (Canada); NAOC (China); CEA, (France); CNES, (France); CNRS,
(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, (UK); UKSA
(UK); NASA (USA); ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI,
(Italy); CNR, (Italy); INAF (Italy); DoE (USA); STFC (UK); CSIC (Spain);
MICINN (Spain); JA (Spain); Tekes (Finland); AoF (Finland); CSC
(Finland); DLR (Germany); MPG (Germany); DTU Space (Denmark); SER/SSO
(Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ESA
(France); CNR (Italy); PRACE (EU); UK STFC; UKSA; Science and Technology
Facilities Council [ST/I000976/1]; ASI/INAF [I/072/09/0]; Italian Space
Agency (ASI Herschel Science Contract) [I/005/07/0]
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). 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). 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). The data
presented in this paper will be released through the Herschel Database
in Marseille HeDaM (hedam.oamp.fr/HerMES). The authors would like to
thank Mattia Negrello for the provision of Fig. 14. This work is funded
in part by the UK STFC and UKSA. SJO, LW and AS acknowledge support from
the Science and Technology Facilities Council [grant number
ST/I000976/1], GdZ acknowledges financial support by ASI/INAF agreement
I/072/09/0. Lucia Marchetti, and Mattia Vaccari were supported by the
Italian Space Agency (ASI Herschel Science Contract I/005/07/0).
NR 75
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PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2014
VL 439
IS 2
BP 1193
EP 1211
DI 10.1093/mnras/stt2253
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE6OS
UT WOS:000334114000001
ER
PT J
AU Matsuura, M
Bernard-Salas, J
Evans, TL
Volk, KM
Hrivnak, BJ
Sloan, GC
Chu, YH
Gruendl, R
Kraemer, KE
Peeters, E
Szczerba, R
Wood, PR
Zijlstra, AA
Hony, S
Ita, Y
Kamath, D
Lagadec, E
Parker, QA
Reid, WA
Shimonishi, T
Van Winckel, H
Woods, PM
Kemper, F
Meixner, M
Otsuka, M
Sahai, R
Sargent, BA
Hora, JL
McDonald, I
AF Matsuura, Mikako
Bernard-Salas, Jeronimo
Evans, T. Lloyd
Volk, Kevin M.
Hrivnak, Bruce J.
Sloan, G. C.
Chu, You-Hua
Gruendl, Robert
Kraemer, Kathleen E.
Peeters, Els
Szczerba, R.
Wood, P. R.
Zijlstra, Albert A.
Hony, S.
Ita, Yoshifusa
Kamath, Devika
Lagadec, Eric
Parker, Quentin A.
Reid, Warren A.
Shimonishi, Takashi
Van Winckel, H.
Woods, Paul M.
Kemper, F.
Meixner, Margaret
Otsuka, M.
Sahai, R.
Sargent, B. A.
Hora, J. L.
McDonald, Iain
TI Spitzer Space Telescope spectra of post-AGB stars in the Large
Magellanic Cloud - polycyclic aromatic hydrocarbons at low metallicities
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: AGB and post-AGB; circumstellar matter; galaxies: individual:
Large Magellanic Cloud; infrared: stars
ID R-CORONAE-BOREALIS; YOUNG STELLAR OBJECTS; 21 MU-M; RICH PROTOPLANETARY
NEBULAE; ASYMPTOTIC GIANT BRANCH; LONG-PERIOD VARIABLES; EXTREME CARBON
STARS; WOLF-RAYET STARS; INFRARED-EMISSION BANDS; LUMINOUS BLUE
VARIABLES
AB This paper reports variations of polycyclic aromatic hydrocarbons (PAHs) features that were found in Spitzer Space Telescope spectra of carbon-rich post-asymptotic giant branch (post-AGB) stars in the Large Magellanic Cloud (LMC). The paper consists of two parts. The first part describes our Spitzer spectral observing programme of 24 stars including post-AGB candidates. The latter half of this paper presents the analysis of PAH features in 20 carbon-rich post-AGB stars in the LMC, assembled from the Spitzer archive as well as from our own programme. We found that five post-AGB stars showed a broad feature with a peak at 7.7 mu m, that had not been classified before. Further, the 10-13 mu m PAH spectra were classified into four classes, one of which has three broad peaks at 11.3, 12.3 and 13.3 mu m rather than two distinct sharp peaks at 11.3 and 12.7 mu m, as commonly found in H ii regions. Our studies suggest that PAHs are gradually processed while the central stars evolve from post-AGB phase to planetary nebulae, changing their composition before PAHs are incorporated into the interstellar medium. Although some metallicity dependence of PAH spectra exists, the evolutionary state of an object is more significant than its metallicity in determining the spectral characteristics of PAHs for LMC and Galactic post-AGB stars.
C1 [Matsuura, Mikako; Woods, Paul M.] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England.
[Bernard-Salas, Jeronimo] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Bernard-Salas, Jeronimo] Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Evans, T. Lloyd] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Volk, Kevin M.; Meixner, Margaret] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Hrivnak, Bruce J.] Valparaiso Univ, Dept Phys & Astron, Valparaiso, IN 46383 USA.
[Sloan, G. C.; Lagadec, Eric] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Chu, You-Hua; Gruendl, Robert] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Kraemer, Kathleen E.] Boston Coll, Inst Sci Res, Newton, MA 02459 USA.
[Peeters, Els] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Peeters, Els] SETI Inst, Mountain View, CA 94043 USA.
[Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland.
[Wood, P. R.; Kamath, Devika] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Zijlstra, Albert A.; McDonald, Iain] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Hony, S.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Ita, Yoshifusa] Tohoku Univ, Grad Sch Sci, Astron Inst, Sendai, Miyagi 9808578, Japan.
[Parker, Quentin A.; Reid, Warren A.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Parker, Quentin A.] Macquarie Univ, Res Ctr Astron Astrophys & Astrophoton MQAAAstro, N Ryde, NSW 2109, Australia.
[Parker, Quentin A.] Australian Astron Observ, Epping, NSW 2121, Australia.
[Shimonishi, Takashi] Kobe Univ, Grad Sch Sci, Dept Earth & Planetary Sci, Nada Kobe 6578501, Japan.
[Van Winckel, H.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Woods, Paul M.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Kemper, F.; Otsuka, M.] AS NTU, Acad Sin, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sargent, B. A.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
[Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Matsuura, M (reprint author), Univ London Univ Coll, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
EM mikako@star.ucl.ac.uk
RI Kemper, Francisca/D-8688-2011; Woods, Paul/E-6926-2011;
OI Kemper, Francisca/0000-0003-2743-8240; Woods, Paul/0000-0003-4340-3590;
Hora, Joseph/0000-0002-5599-4650; Kraemer, Kathleen/0000-0002-2626-7155;
Van Winckel, Hans/0000-0001-5158-9327
FU NASA [1378453]; National Aeronautics and Space Administration; National
Science Foundation; Marie Curie Actions IRSES of EU [269193]; Polish NCN
[2011/01/B/ST9/02031]; National Science Council
[NSC100-2112-M-001-023-MY3]; NASA; Spitzer Guest Observer programme
FX MM thanks Professor I. D. Howarth for his inputs about the
classifications of high-mass stars. We thank Dr J. P. Searle for
providing the Herschel measurements of IRAS 05189-7008 fluxes. Support
for this research was provided by NASA through contract 1378453 issued
by JPL/Caltech. 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 the SIMBAD data base, operated at CDS, Strasbourg, France.
RSz acknowledges support from Marie Curie Actions IRSES (project No.
269193) of EU and from Polish NCN grant 2011/01/B/ST9/02031. FK
acknowledges financial support from the National Science Council under
grant number NSC100-2112-M-001-023-MY3. RS's contribution to the
research described here was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA, and supported via an award issued by JPL/Caltech in support of his
Spitzer Guest Observer programme.
NR 135
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2014
VL 439
IS 2
BP 1472
EP 1493
DI 10.1093/mnras/stt2495
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE6OS
UT WOS:000334114000016
ER
PT J
AU Marsden, D
Gralla, M
Marriage, TA
Switzer, ER
Partridge, B
Massardi, M
Morales, G
Addison, G
Bond, JR
Crichton, D
Das, S
Devlin, M
Dunner, R
Hajian, A
Hilton, M
Hincks, A
Hughes, JP
Irwin, K
Kosowsky, A
Menanteau, F
Moodley, K
Niemack, M
Page, L
Reese, ED
Schmitt, B
Sehgal, N
Sievers, J
Staggs, S
Swetz, D
Thornton, R
Wollack, E
AF Marsden, Danica
Gralla, Megan
Marriage, Tobias A.
Switzer, Eric R.
Partridge, Bruce
Massardi, Marcella
Morales, Gustavo
Addison, Graeme
Bond, J. Richard
Crichton, Devin
Das, Sudeep
Devlin, Mark
Duenner, Rolando
Hajian, Amir
Hilton, Matt
Hincks, Adam
Hughes, John P.
Irwin, Kent
Kosowsky, Arthur
Menanteau, Felipe
Moodley, Kavilan
Niemack, Michael
Page, Lyman
Reese, Erik D.
Schmitt, Benjamin
Sehgal, Neelima
Sievers, Jonathan
Staggs, Suzanne
Swetz, Daniel
Thornton, Robert
Wollack, Edward
TI The Atacama Cosmology Telescope: dusty star-forming galaxies and active
galactic nuclei in the Southern survey
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: numerical; surveys; galaxies: active; galaxies: high-redshift
ID COEVAL OBSERVATIONS PROJECT; CLERK MAXWELL TELESCOPE; SOURCE CATALOG;
EXTRAGALACTIC SOURCES; POLE TELESCOPE; BOLOMETER CAMERA; BLAZAR
SEQUENCE; NUMBER COUNTS; BRIGHTNESS TEMPERATURES; REDSHIFT DISTRIBUTION
AB We present a catalogue of 191 extragalactic sources detected by the Atacama Cosmology Telescope (ACT) at 148 and/or 218 GHz in the 2008 Southern survey. Flux densities span 14 -1700 mJy, and we use source spectral indices derived using ACT-only data to divide our sources into two subpopulations: 167 radio galaxies powered by central active galactic nuclei (AGN) and 24 dusty star-forming galaxies (DSFGs). We cross-identify 97 per cent of our sources (166 of the AGN and 19 of the DSFGs) with those in currently available catalogues. When combined with flux densities from the Australia Telescope 20 GHz survey and follow-up observations with the Australia Telescope Compact Array, the synchrotron-dominated population is seen to exhibit a steepening of the slope of the spectral energy distribution from 20 to 148 GHz, with the trend continuing to 218 GHz. The ACT dust-dominated source population has a median spectral index, alpha(148-218), of 3.7(-0.86)(+0.62), and includes both local galaxies and sources with redshift around 6. Dusty sources with no counterpart in existing catalogues likely belong to a recently discovered subpopulation of DSFGs lensed by foreground galaxies or galaxy groups.
C1 [Marsden, Danica] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Marsden, Danica; Devlin, Mark; Reese, Erik D.; Schmitt, Benjamin] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Gralla, Megan; Marriage, Tobias A.; Crichton, Devin] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Switzer, Eric R.; Wollack, Edward] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Massardi, Marcella] Astron Observ Padova, INAF, I-35122 Padua, Italy.
[Morales, Gustavo; Duenner, Rolando] Pontificia Univ Catolica Chile, Fac Fis, Dept Astronomia & Astrofis, Santiago 22, Chile.
[Addison, Graeme] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T IZ4, Canada.
[Bond, J. Richard; Hajian, Amir; Hincks, Adam; Sievers, Jonathan] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA.
[Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA.
[Hilton, Matt; Moodley, Kavilan; Sievers, Jonathan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Hughes, John P.; Menanteau, Felipe] State Univ New Jersey, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Irwin, Kent; Swetz, Daniel] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Niemack, Michael] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Page, Lyman; Sievers, Jonathan; Staggs, Suzanne] Princeton Univ, Jadwin Hall, Princeton, NJ 08544 USA.
[Sehgal, Neelima] SUNY Stony Brook, Phys & Astron Dept, Stony Brook, NY 11794 USA.
[Thornton, Robert] West Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA.
RP Marsden, D (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
EM danica@physics.ucsb.edu
RI Wollack, Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Menanteau,
Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074
FU US National Science Foundation [AST-0408698, AST-0965625]; Princeton
University; University of Pennsylvania; Canada Foundation for Innovation
(CFI); NSF Physics Frontier Center [PHY-0114422]; SciNet; Canada
Foundation for Innovation (CFI) under the Compute Canada; Government of
Ontario; Ontario Research Fund Research Excellence; University of
Toronto; Comision Nacional de Investigacion Cientifica y Tecnologica de
Chile (CONICYT); Commonwealth of Australia; National Aeronautics and
Space Administration; [PHY-0355328]; [PHY-0855887]; [PHY-1214379];
[AST-0707731]; [PIRE-0507768]; [OISE-0530095]
FX This work was supported by the US National Science Foundation through
awards AST-0408698 and AST-0965625 for the ACT project, and PHY-0355328,
PHY-0855887, PHY-1214379, AST-0707731 and PIRE-0507768 (award number
OISE-0530095). Funding was also provided by Princeton University, the
University of Pennsylvania and a Canada Foundation for Innovation (CFI)
award to UBC. ES acknowledges support by NSF Physics Frontier Center
grant PHY-0114422 to the Kavli Institute of Cosmological Physics. The
PIRE programme enabled this research through exchanges between Chile,
South Africa, Spain and the US. Computations were performed on the GPC
supercomputer at the SciNet HPC Consortium. SciNet is funded by SciNet
is funded by the Canada Foundation for Innovation (CFI) under the
auspices of Compute Canada, the Government of Ontario, the Ontario
Research Fund Research Excellence and the University of Toronto. Data
acquisition electronics were developed with assistance from the CFI. ACT
operates in the Parque Astronmico Atacama in northern Chile under the
auspices of the Comision Nacional de Investigacion Cientifica y
Tecnologica de Chile (CONICYT).; We thank the staff at the Australia
Telescope Compact Array site, Narrabri (NSW), for the valuable support
they provide in running the telescope. 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 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.
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PD APR
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE6OS
UT WOS:000334114000021
ER
PT J
AU Ng, C
Bailes, M
Bates, SD
Bhat, NDR
Burgay, M
Burke-Spolaor, S
Champion, DJ
Coster, P
Johnston, S
Keith, MJ
Kramer, M
Levin, L
Petroff, E
Possenti, A
Stappers, BW
van Straten, W
Thornton, D
Tiburzi, C
Bassa, CG
Freire, PCC
Guillemot, L
Lyne, AG
Tauris, TM
Shannon, RM
Wex, N
AF Ng, C.
Bailes, M.
Bates, S. D.
Bhat, N. D. R.
Burgay, M.
Burke-Spolaor, S.
Champion, D. J.
Coster, P.
Johnston, S.
Keith, M. J.
Kramer, M.
Levin, L.
Petroff, E.
Possenti, A.
Stappers, B. W.
van Straten, W.
Thornton, D.
Tiburzi, C.
Bassa, C. G.
Freire, P. C. C.
Guillemot, L.
Lyne, A. G.
Tauris, T. M.
Shannon, R. M.
Wex, N.
TI The High Time Resolution Universe pulsar survey - X. Discovery of four
millisecond pulsars and updated timing solutions of a further 12
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: neutron; pulsars: general; pulsars: individual: PSR J1017-7156;
pulsars: individual: PSR J1543-5149; pulsars: individual: PSR
J1801-3210; pulsars: individual: PSR J1811-2405
ID LARGE-AREA TELESCOPE; GAMMA-RAY PULSARS; BINARY PULSARS; NEUTRON-STAR;
GRAVITATIONAL-RADIATION; EQUIVALENCE PRINCIPLES; GALACTIC DISTRIBUTION;
INITIAL DISCOVERIES; RADIO-EMISSION; FREE-ELECTRONS
AB We report on the discovery of four millisecond pulsars (MSPs) in the High Time Resolution Universe (HTRU) pulsar survey being conducted at the Parkes 64 m radio telescope. All four MSPs are in binary systems and are likely to have white dwarf companions. In addition, we present updated timing solutions for 12 previously published HTRU MSPs, revealing new observational parameters such as five proper motion measurements and significant temporal dispersion measure variations in PSR J1017-7156. We discuss the case of PSR J1801-3210, which shows no significant period derivative P after four years of timing data. Our best-fitting solution shows a P of the order of 10(-23), an extremely small number compared to that of a typical MSP. However, it is likely that the pulsar lies beyond the Galactic Centre, and an unremarkable intrinsic P is reduced to close to zero by the Galactic potential acceleration. Furthermore, we highlight the potential to employ PSR J1801-3210 in the strong equivalence principle test due to its wide and circular orbit. In a broader comparison with the known MSP population, we suggest a correlation between higher mass functions and the presence of eclipses in 'very low mass binary pulsars', implying that eclipses are observed in systems with high orbital inclinations. We also suggest that the distribution of the total mass of binary systems is inversely related to the Galactic height distribution. Finally, we report on the first detection of PSRs J1543-5149 and J1811-2404 as gamma-ray pulsars.
C1 [Ng, C.; Champion, D. J.; Kramer, M.; Freire, P. C. C.; Guillemot, L.; Tauris, T. M.; Wex, N.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Bailes, M.; Bhat, N. D. R.; Coster, P.; Petroff, E.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Bailes, M.; Bhat, N. D. R.; Petroff, E.; van Straten, W.] Swinburne Univ Technol, ARC Ctr Excellence All Sky Astrophys CAASTRO, Hawthorn, Vic 3122, Australia.
[Bates, S. D.; Levin, L.] 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.; Possenti, A.; Tiburzi, C.] Osservatorio Astron Cagliari, I-09012 Capoterra, CA, Italy.
[Burke-Spolaor, S.] NASA Jet Prop Lab, Pasadena, CA 91106 USA.
[Coster, P.; Johnston, S.; Keith, M. J.; Petroff, E.; Thornton, D.; Shannon, R. M.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Kramer, M.; Stappers, B. W.; Thornton, D.; Bassa, C. G.; Lyne, A. G.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Tiburzi, C.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy.
[Guillemot, L.] Univ Orleans, CNRS, Lab Phys & Chim Environm & Espace, F-45071 Orleans 02, France.
[Tauris, T. M.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
RP Ng, C (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM cherryng@mpifr-bonn.mpg.de
OI Champion, David/0000-0003-1361-7723; Shannon, Ryan/0000-0002-7285-6348;
Burgay, Marta/0000-0002-8265-4344; van Straten,
Willem/0000-0003-2519-7375
FU Commonwealth of Australia; Parkes Pulsar Timing Array Project [P456];
International Max Planck Research School (IMPRS) for Astronomy and
Astrophysics at the Universities of Bonn and Cologne
FX 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. A large amount of the timing data for PSR
J1017-7156 has been taken as part of the Parkes Pulsar Timing Array
Project P456.; The authors would like to thank Patrick Lazarus for
providing an automated RFI cleaning routine, Dominic Schnitzeler for
useful discussions on pulsar distances, Joris Verbiest for his expertise
on the use of TEMPO2, Charlotte Sobey and Gregory Desvignes for advices
on data calibration, Kejia Lee for his help in plotting Fig. 7, Chris
Flynn for sharing his knowledge on Galactic stellar density, Megan
DeCesar from the Fermi collaboration for reviewing the paper and
providing many constructive suggestions, and Lijing Shao for carefully
reading the manuscripts. CN was supported for this research through a
stipend from the International Max Planck Research School (IMPRS) for
Astronomy and Astrophysics at the Universities of Bonn and Cologne.
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SC Astronomy & Astrophysics
GA AE6OS
UT WOS:000334114000038
ER
PT J
AU Delvecchio, I
Gruppioni, C
Pozzi, F
Berta, S
Zamorani, G
Cimatti, A
Lutz, D
Scott, D
Vignali, C
Cresci, G
Feltre, A
Cooray, A
Vaccari, M
Fritz, J
Le Floc'h, E
Magnelli, B
Popesso, P
Oliver, S
Bock, J
Carollo, M
Contini, T
Le Fevre, O
Lilly, S
Mainieri, V
Renzini, A
Scodeggio, M
AF Delvecchio, I.
Gruppioni, C.
Pozzi, F.
Berta, S.
Zamorani, G.
Cimatti, A.
Lutz, D.
Scott, D.
Vignali, C.
Cresci, G.
Feltre, A.
Cooray, A.
Vaccari, M.
Fritz, J.
Le Floc'h, E.
Magnelli, B.
Popesso, P.
Oliver, S.
Bock, J.
Carollo, M.
Contini, T.
Le Fevre, O.
Lilly, S.
Mainieri, V.
Renzini, A.
Scodeggio, M.
TI Tracing the cosmic growth of supermassive black holes to z similar to 3
with Herschel(star)
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: nuclei; infrared: galaxies
ID ACTIVE GALACTIC NUCLEI; DEEP-FIELD-SOUTH; SPECTRAL ENERGY-DISTRIBUTIONS;
STAR-FORMATION HISTORY; ULTRALUMINOUS INFRARED GALAXIES; RAY LUMINOSITY
FUNCTION; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; X-RAY;
XMM-NEWTON
AB We study a sample of Herschel selected galaxies within the Great Observatories Origins Deep Survey-South and the Cosmic Evolution Survey fields in the framework of the Photodetector Array Camera and Spectrometer (PACS) Evolutionary Probe project. Starting from the rich multiwavelength photometric data sets available in both fields, we perform a broad-band spectral energy distribution decomposition to disentangle the possible active galactic nucleus (AGN) contribution from that related to the host galaxy. We find that 37 per cent of the Herschel-selected sample shows signatures of nuclear activity at the 99 per cent confidence level. The probability of revealing AGN activity increases for bright (L1-1000 > 10(11) L-circle dot) star-forming galaxies at z > 0.3, becoming about 80 per cent for the brightest (L1-1000 > 10(12) L-circle dot) infrared (IR) galaxies at z >= 1. Finally, we reconstruct the AGN bolometric luminosity function and the supermassive black hole growth rate across cosmic time up to z similar to 3 from a far-IR perspective. This work shows general agreement with most of the panchromatic estimates from the literature, with the global black hole growth peaking at z similar to 2 and reproducing the observed local black hole mass density with consistent values of the radiative efficiency epsilon(rad) (similar to 0.07).
C1 [Delvecchio, I.; Pozzi, F.; Cimatti, A.; Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy.
[Gruppioni, C.; Zamorani, G.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Berta, S.; Lutz, D.; Popesso, P.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Cresci, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Feltre, A.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy.
[Feltre, A.; Mainieri, V.] ESO, D-85748 Garching, Germany.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Cooray, A.; Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa.
[Fritz, J.] Vakgrp Fys Sterrenkunde Univ, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Le Floc'h, E.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Magnelli, B.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Oliver, S.] Univ Sussex, Dept Phys & Astron, Astron Ctr, Brighton BN1 9QH, E Sussex, England.
[Bock, J.] CALTECH, Pasadena, CA 91125 USA.
[Carollo, M.; Lilly, S.] ETH Honggerberg, Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland.
[Contini, T.] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Le Fevre, O.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Renzini, A.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[Scodeggio, M.] INAF IASF Milano, I-20133 Milan, Italy.
RP Delvecchio, I (reprint author), Univ Bologna, Dipartimento Fis & Astron, Via Ranzani 1, I-40127 Bologna, Italy.
EM ivan.delvecchio@unibo.it
RI Vignali, Cristian/J-4974-2012; Vaccari, Mattia/R-3431-2016;
OI Cresci, Giovanni/0000-0002-5281-1417; Vignali,
Cristian/0000-0002-8853-9611; Vaccari, Mattia/0000-0002-6748-0577;
Scodeggio, Marco/0000-0002-2282-5850; Gruppioni,
Carlotta/0000-0002-5836-4056; Scott, Douglas/0000-0002-6878-9840;
Zamorani, Giovanni/0000-0002-2318-301X; Delvecchio,
Ivan/0000-0001-8706-2252
FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany);
ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA
(France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB
(Sweden); STFC (UK); UKSA (UK); NASA (USA)
FX This paper uses data from Herschel's photometers PACS and SPIRE. PACS
has been developed by a consortium of institutes led by MPE (Germany)
and including: UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM
(France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy) and
IAC (Spain). This development has been supported by the funding agencies
BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany),
ASI/INAF (Italy), and CICYT/MCYT (Spain). 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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SC Astronomy & Astrophysics
GA AE6PB
UT WOS:000334114900038
ER
PT J
AU Szypryt, P
Duggan, GE
Mazin, BA
Meeker, SR
Strader, MJ
van Eyken, JC
Marsden, D
O'Brien, K
Walter, AB
Ulbricht, G
Prince, TA
Stoughton, C
Bumble, B
AF Szypryt, P.
Duggan, G. E.
Mazin, B. A.
Meeker, S. R.
Strader, M. J.
van Eyken, J. C.
Marsden, D.
O'Brien, K.
Walter, A. B.
Ulbricht, G.
Prince, T. A.
Stoughton, C.
Bumble, B.
TI Direct detection of SDSS J0926+3624 orbital expansion with ARCONS
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: close; binaries: eclipsing; stars: individual: SDSS
J0926+3624; cataclysmic variables; white dwarfs
ID AM CVN STARS; CATACLYSMIC VARIABLES; BINARIES
AB AM Canum Venaticorum (AM CVn) stars belong to a class of ultracompact, short-period binaries with spectra dominated largely by helium. SDSS J0926+3624 is of particular interest as it is the first observed eclipsing AM CVn system. We observed SDSS J0926+3624 with the Array Camera for Optical to Near-IR Spectrophotometry (ARCONS) at the Palomar 200 ' telescope. ARCONS uses a relatively new type of energy-resolved photon counters called Microwave Kinetic Inductance Detectors. ARCONS, sensitive to radiation from 350 to 1100 nm, has a time resolution of several microseconds and can measure the energy of a photon to similar to 10 per cent. We present the light curves for these observations and examine changes in orbital period from prior observations. Using a quadratic ephemeris model, we measure a period rate of change P = (3.07 +/- 0.56) x 10(-13). In addition, we use the high timing resolution of ARCONS to examine the system's high-frequency variations and search for possible quasi-periodic oscillations (QPOs). Finally, we use the instrument's spectral resolution to examine the light curves in various wavelength bands. We do not find any high-frequency QPOs or significant spectral variability throughout an eclipse.
C1 [Szypryt, P.; Duggan, G. E.; Mazin, B. A.; Meeker, S. R.; Strader, M. J.; van Eyken, J. C.; Marsden, D.; Walter, A. B.; Ulbricht, G.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Duggan, G. E.; Prince, T. A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[O'Brien, K.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Stoughton, C.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Bumble, B.] NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Szypryt, P (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
EM pszypryt@physics.ucsb.edu
RI Mazin, Ben/B-8704-2011; Ulbricht, Gerhard/P-7487-2016
OI Mazin, Ben/0000-0003-0526-1114; Ulbricht, Gerhard/0000-0002-6497-3763
FU NASA [NNX11AD55G, NNX10AF58G]; NASA Office of the Chief Technologist's
Space Technology Research Fellowship, NASA [NNX11AN29H]; Keck Institute
for Space Studies; Fermi Research Alliance, LLC [De-AC02-07CH11359]
FX The MKID detectors used in this work were developed under NASA grant
NNX11AD55G, and the readout was partially developed under NASA grant
NNX10AF58G. SRM was supported by a NASA Office of the Chief
Technologist's Space Technology Research Fellowship, NASA grant
NNX11AN29H. This work was partially supported by the Keck Institute for
Space Studies. Fermilab is operated by Fermi Research Alliance, LLC
under Contract no. De-AC02-07CH11359 with the United States Department
of Energy. The authors would like to thank Shri Kulkarni, Director of
the Caltech Optical Observatories for facilitating this project, as well
as the excellent staff of the Palomar Observatory. This project also
greatly benefitted from the support of Mike Werner, Paul Goldsmith, and
Jonas Zmuidzinas at JPL.
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SC Astronomy & Astrophysics
GA AE6PB
UT WOS:000334114900040
ER
PT J
AU Matt, G
Marinucci, A
Guainazzi, M
Brenneman, LW
Elvis, M
Lohfink, A
Arevalo, P
Boggs, SE
Cappi, M
Christensen, FE
Craig, WW
Fabian, AC
Fuerst, F
Hailey, CJ
Harrison, FA
Parker, M
Reynolds, CS
Stern, D
Walton, DJ
Zhang, WW
AF Matt, G.
Marinucci, A.
Guainazzi, M.
Brenneman, L. W.
Elvis, M.
Lohfink, A.
Arevalo, P.
Boggs, S. E.
Cappi, M.
Christensen, F. E.
Craig, W. W.
Fabian, A. C.
Fuerst, F.
Hailey, C. J.
Harrison, F. A.
Parker, M.
Reynolds, C. S.
Stern, D.
Walton, D. J.
Zhang, W. W.
TI The soft-X-ray emission of Ark 120. XMM-Newton, NuSTAR, and the
importance of taking the broad view
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; galaxies: active; galaxies: individual: Ark
120
ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; LINE REGION SIZES; SUZAKU
OBSERVATIONS; CENTRAL MASSES; SKY SURVEY; SPECTRA; EXCESS;
PHOTOIONIZATION; SEYFERT-1
AB We present simultaneous XMM-Newton and NuSTAR observations of the 'bare' Seyfert 1 galaxy, Ark 120, a system in which ionized absorption is absent. The NuSTAR hard-X-ray spectral coverage allows us to constrain different models for the excess soft-X-ray emission. Among phenomenological models, a cutoff power law best explains the soft-X-ray emission. This model likely corresponds to Comptonization of the accretion disc seed UV photons by a population of warm electrons: using Comptonization models, a temperature of similar to 0.3 keV and an optical depth of similar to 13 are found. If the UV-to-X-ray optxagnf model is applied, the UV fluxes from the XMM-Newton Optical Monitor suggest an intermediate black hole spin. Contrary to several other sources observed by NuSTAR, no high-energy cutoff is detected with a lower limit of 190 keV.
C1 [Matt, G.; Marinucci, A.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Guainazzi, M.] European Space Astron Ctr ESA, E-28080 Madrid, Spain.
[Brenneman, L. W.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lohfink, A.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Arevalo, P.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 22, Chile.
[Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Cappi, M.] IASF Bologna, INAF, I-40129 Bologna, Italy.
[Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Fabian, A. C.; Parker, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Fuerst, F.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Matt, G (reprint author), Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy.
EM matt@fis.uniroma3.it
RI Boggs, Steven/E-4170-2015; Cappi, Massimo/F-4813-2015;
OI Boggs, Steven/0000-0001-9567-4224; Cappi, Massimo/0000-0001-6966-8920
FU National Aeronautics and Space Administration; ESA Member States; USA
(NASA); Italian Space Agency under grant ASI/INAF [I/037/12/0-011/13];
European Union [312789]
FX We thank the anonymous referee for useful comments which helped us to
improve the clarity of the paper, and Chris Done for comments and
advices on the OPTXAGNF model. This work has 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
NUSTARDAS jointly developed by the ASI Science Data Center (ASDC, Italy)
and the California Institute of Technology (USA). The work is also based
on observations obtained with XMM-Newton, an ESA science mission with
instruments and contributions directly funded by ESA Member States and
the USA (NASA). GM and AM acknowledge financial support from Italian
Space Agency under grant ASI/INAF I/037/12/0-011/13 and from the
European Union Seventh Framework Programme (FP7/2007-2013) under grant
agreement n. 312789.
NR 32
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PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2014
VL 439
IS 3
BP 3016
EP 3021
DI 10.1093/mnras/stu159
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE6PB
UT WOS:000334114900063
ER
PT J
AU Maccarone, TJ
Lehmer, BD
Leyder, JC
Antoniou, V
Hornschemeier, A
Ptak, A
Wik, D
Zezas, A
AF Maccarone, Thomas J.
Lehmer, Bret D.
Leyder, J. C.
Antoniou, Vallia
Hornschemeier, Ann
Ptak, Andrew
Wik, Daniel
Zezas, Andreas
TI A new candidate Wolf-Rayet X-ray binary in NGC 253
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: Wolf-Rayet; galaxies: individual: NGC 253; galaxies: starburst;
X-rays: binaries
ID STAR-FORMATION HISTORY; DOUBLE BLACK-HOLE; GRAVITATIONAL-RADIATION;
GLOBULAR-CLUSTER; IC-10 X-1; MASS; ACCRETION; EVOLUTION; GALAXIES;
VARIABILITY
AB We have discovered a persistent, but highly variable X-ray source in the nearby starburst galaxy NGC 253. The source varies at the level of a factor of about 5 in count rate on time-scales of a few hours. Two long observations of the source with Chandra and XMM-Newton show suggestive evidence for the source having a period of about 14-15 hours, but the time sampling in existing data is insufficient to allow a firm determination that the source is periodic. Given the amplitude of variation and the location in a nuclear starburst, the source is likely to be a Wolf-Rayet X-ray binary, with the tentative period being the orbital period of the system. In light of the fact that we have demonstrated that careful examination of the variability of moderately bright X-ray sources in nearby galaxies can turn up candidate Wolf-Rayet X-ray binaries, we discuss the implications of Wolf-Rayet X-ray binaries for predictions of the gravitational wave source event rate, and, potentially, interpretations of the events.
C1 [Maccarone, Thomas J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
[Lehmer, Bret D.; Ptak, Andrew] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Lehmer, Bret D.; Leyder, J. C.; Hornschemeier, Ann; Ptak, Andrew; Wik, Daniel] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Leyder, J. C.] European Space Agcy, European Space Astron Ctr, E-28691 Madrid, Spain.
[Antoniou, Vallia] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Antoniou, Vallia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zezas, Andreas] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece.
RP Maccarone, TJ (reprint author), Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
EM thomas.maccarone@ttu.edu
RI Zezas, Andreas/C-7543-2011; Antoniou, Vallia/E-3837-2013
OI Zezas, Andreas/0000-0001-8952-676X; Antoniou, Vallia/0000-0001-7539-1593
NR 60
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PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2014
VL 439
IS 3
BP 3064
EP 3072
DI 10.1093/mnras/stu167
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE6PB
UT WOS:000334114900068
ER
PT J
AU Wolters, SD
Weissman, PR
Christou, A
Duddy, SR
Lowry, SC
AF Wolters, Stephen D.
Weissman, Paul R.
Christou, Apostolis
Duddy, Samuel R.
Lowry, Stephen C.
TI Spectral similarity of unbound asteroid pairs
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; minor planets, asteroids: general
ID SPECTROSCOPIC SURVEY; PHASE-II; ORIGIN
AB Infrared (IR) spectroscopy between 0.8 and 2.5 mu has been obtained for both components of three unbound asteroid pairs, using the NASA Infrared Telescope Facility with the SpeX instrument. Pair primary (2110) Moore-Sitterly is classified as an S-type following the Bus-DeMeo taxonomy; the classification for secondary (44612) 1999 RP27 is ambiguous: S/Sq/Q/K/L-type. Primary (10484) Hecht and secondary (44645) 1999 RC118 are classified as V-types. IR spectra for Moore-Sitterly and Hecht are each linked with available visual photometry. The classifications for primary (88604) 2001 QH293 and (60546) 2000 EE85 are ambiguous: S/Sq/Q/K/L-type. Subtle spectral differences between them suggest that the primary may have more weathered material on its surface. Dynamical integrations have constrained the ages of formation: 2110-44612 > 782 kyr; 10484-44645 = 348 (+823,-225) kyr; 88604-60546 = 925 (+842,-754) kyr. The spectral similarity of seven complete pairs is ranked in comparison with nearby background asteroids. Two pairs, 17198-229056 and 19289-278067, have significantly different spectra between the components, compared to the similarity of spectra in the background population. The other pairs are closer than typical, supporting an interpretation of each pair's formation from a common parent body.
C1 [Wolters, Stephen D.; Weissman, Paul R.] CALTECH, Planetary Sci Sect, Jet Prop Lab, Pasadena, CA 91109 USA.
[Christou, Apostolis] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Duddy, Samuel R.; Lowry, Stephen C.] Univ Kent, Sch Phys Sci, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England.
RP Wolters, SD (reprint author), Open Univ, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
EM s.d.wolters@open.ac.uk
FU University of Hawaii [NNX-08AE38A]; National Aeronautics and Space
Administration; Science Mission Directorate; NASA; National Science
Foundation [0506716, 0907766]; NASA [NAG5-12355, 09-NEOO009-0001];
Northern Ireland Department of Culture, Arts and Leisure (DCAL); SFI/HEA
Irish Centre for High-End Computing (ICHEC)
FX Visiting Astronomer at the IRTF, which is operated by the University of
Hawaii under Cooperative Agreement no. NNX-08AE38A with the National
Aeronautics and Space Administration, Science Mission Directorate,
Planetary Astronomy Program. A part of this work was performed at the
Jet Propulsion Laboratory under a contract with NASA. Taxonomic-type
results presented in this work were determined, in part, using a
Bus-DeMeo Taxonomy Classification Web tool by Stephen M. Slivan,
developed at MIT with the support of National Science Foundation Grant
0506716 and NASA Grant NAG5-12355. Part of the data utilized in this
publication were obtained and made available by the MIT-UH-IRTF Joint
Campaign for NEO Reconnaissance. The MIT component of this work is
supported by NASA grant 09-NEOO009-0001, and by the National Science
Foundation under grants nos 0506716 and 0907766. Astronomical research
at the Armagh Observatory is funded by the Northern Ireland Department
of Culture, Arts and Leisure (DCAL). We thank an anonymous referee for
many helpful comments that improved this manuscript. AC acknowledges the
SFI/HEA Irish Centre for High-End Computing (ICHEC) for the provision of
computational facilities and support.
NR 26
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U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2014
VL 439
IS 3
BP 3085
EP 3093
DI 10.1093/mnras/stu171
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE6PB
UT WOS:000334114900070
ER
PT J
AU Fairen, AG
Stokes, CR
Davies, NS
Schulze-Makuch, D
Rodriguez, JAP
Davila, AF
Uceda, ER
Dohm, JM
Baker, VR
Clifford, SM
McKay, CP
Squyres, SW
AF Fairen, Alberto G.
Stokes, Chris R.
Davies, Neil S.
Schulze-Makuch, Dirk
Rodriguez, J. Alexis P.
Davila, Alfonso F.
Uceda, Esther R.
Dohm, James M.
Baker, Victor R.
Clifford, Stephen M.
Mckay, Christopher P.
Squyres, Steven W.
TI A cold hydrological system in Gale crater, Mars
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Gale crater; Glacial/periglacial modification; Glacio-fluvial
activity; Fluvial erosion; Ground ice
ID ART. NO. 5111; DICHOTOMY BOUNDARY; ROCK GLACIERS; VALLES MARINERIS;
MELAS-CHASMA; EVOLUTION; ICE; ANTARCTICA; GLACIATION; DRUMLINS
AB Gale crater is a similar to 154-km-diameter impact crater formed during the Late Noachian/Early Hesperian at the dichotomy boundary on Mars. Here we describe potential evidence for ancient glacial, periglacial and fluvial (including glacio-fluvial) activity within Gale crater, and the former presence of ground ice and lakes. Our interpretations are derived from morphological observations using high-resolution datasets, particularly HiRISE and HRSC. We highlight a potential ancient lobate rock-glacier complex in parts of the northern central mound, with further suggestions of glacial activity in the large valley systems towards the southeast central mound. Wide expanses of ancient ground ice may be indicated by evidence for very cohesive ancient river banks and for the polygonal patterned ground common on the crater floor west of the central mound. We extend the interpretation to fluvial and lacustrine activity to the west of the central mound, as recorded by a series of interconnected canyons, channels and a possible lake basin. The emerging picture from our regional landscape analyses is the hypothesis that rock glaciers may have formerly occupied the central mound. The glaciers would have provided the liquid water required for carving the canyons and channels. Associated glaciofluvial activity could have led to liquid water running over ground ice-rich areas on the basin floor, with resultant formation of partially and/or totally ice-covered lakes in parts of the western crater floor. All this hydrologic activity is Hesperian or younger. Following this, we envisage a time of drying, with the generation of polygonal patterned ground and dune development subsequent to the disappearance of the surface liquid and frozen water. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Fairen, Alberto G.; Squyres, Steven W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Fairen, Alberto G.] Ctr Astrobiol, Torrejon De Ardoz 28850, Spain.
[Stokes, Chris R.] Univ Durham, Dept Geog, Durham DH1 3LE, England.
[Davies, Neil S.] Univ Cambridge, Dept Earth Sci, Cambridge CB3 3EQ, England.
[Schulze-Makuch, Dirk] Washington State Univ, Sch Environm, Pullman, WA 99164 USA.
[Rodriguez, J. Alexis P.; Mckay, Christopher P.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Davila, Alfonso F.] SETI Inst, Mountain View, CA 94043 USA.
[Uceda, Esther R.] Univ Autonoma Madrid, Fac Ciencias, E-28049 Madrid, Spain.
[Dohm, James M.] Tokyo Inst Technol, Earth Life Sci Inst, Tokyo 1528551, Japan.
[Dohm, James M.; Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Clifford, Stephen M.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
Lunar & Planetary Inst, Houston, TX 77058 USA.
RP Fairen, AG (reprint author), Cornell Univ, Dept Astron, 426 Space Sci Bldg, Ithaca, NY 14853 USA.
EM agfairen@cornell.edu
RI Stokes, Chris/A-1957-2011; Davila, Alfonso/A-2198-2013;
OI Stokes, Chris/0000-0003-3355-1573; Davila, Alfonso/0000-0002-0977-9909;
Schulze-Makuch, Dirk/0000-0002-1923-9746
FU European Research Council under the European Union's Seventh Framework
Programme [307496]; Philip Leverhulme Prize
FX The authors would like to thank the MRO HiRISE and CTX Teams, and the
MEX HRSC Team, for their efforts in producing the excellent datasets and
observations used here. The research leading to these results has
received funding from the European Research Council under the European
Union's Seventh Framework Programme (FP7/2007-2013), ERC Grant agreement
no. 307496. C. R.S. acknowledges financial support provided by a Philip
Leverhulme Prize. This is LPI Contribution 1778.
NR 84
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U1 2
U2 19
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 APR
PY 2014
VL 93-94
BP 101
EP 118
DI 10.1016/j.pss.2014.03.002
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG2WO
UT WOS:000335278000011
ER
PT J
AU Lipatov, AS
Sittler, EC
Hartle, RE
Cooper, JF
Simpson, DG
AF Lipatov, A. S.
Sittler, E. C., Jr.
Hartle, R. E.
Cooper, J. F.
Simpson, D. G.
TI Titan's plasma environment: 3D hybrid kinetic modeling of the TA flyby
and comparison with CAPS-ELS and RPWS LP observations
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Ionospheres; Atmospheres; Induced magnetospheres; Magnetic barrier;
Alfven wing; Satellites; Pickup ion
ID SOLAR-WIND; SATURNS MAGNETOSPHERE; MHD MODEL; IONOSPHERE; SIMULATION;
SPECTROMETER; T9; ENCOUNTER; VOYAGER-1; EXOSPHERE
AB In this report we discuss the global plasma environment of the TA flyby from the perspective of 3D hybrid modeling. In our model the background, pickup, and ionospheric ions are considered as particles, whereas the electrons are described as a fluid. Inhomogeneous photoionization, electron-impact ionization and charge exchange are included in our model. We also take into account the collisions between the ions and neutrals. Our modeling shows that mass loading of the background plasma (H+, O+) by pickup ions H-2(+), CH4+ and N-2(+) differs from the T9 encounter simulations when O+ ions are not introduced into the background plasma. In our hybrid modeling we use Chamberlain profiles for the atmospheric components. We also include a simple ionosphere model with average mass M=28 amu ions that were generated inside the ionosphere. Titan's interior is considered as a weakly conducting body. Special attention has been paid to comparing the simulated pickup ion density distribution with CAPS-ELS and with RPWS LP observations by the Cassini-Huygens spacecraft along the TA trajectory. Our modeling shows an asymmetry of the ion density distribution and the magnetic field, including the formation of Alfven wing-like structures. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Lipatov, A. S.] NASA, Goddard Space Flight Ctr, GPHI UMBC, Greenbelt, MD 20771 USA.
[Lipatov, A. S.] Moscow Inst Phys & Technol, Fac Problems Phys & Power Engn, Moscow, Russia.
[Sittler, E. C., Jr.; Hartle, R. E.; Cooper, J. F.; Simpson, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lipatov, AS (reprint author), NASA, Goddard Space Flight Ctr, GPHI UMBC, Greenbelt, MD 20771 USA.
EM Alexander.Lipatov-1@nasa.gov; Edward.C.Sittler@nasa.gov;
Richard.E.Hartle@nasa.gov; John.F.Cooper@nasa.gov;
David.G.Simpson@nasa.gov
RI Cooper, John/D-4709-2012
FU NASA Cassini Data Analysis Program [08-CDAP08-0043]; GPHI UMBC
[900-37-172, 670-90-315]; NASA GSFC; NASA Ames Advanced Supercomputing
(NAS) [SMD-09-1124, SMD-13-1517]
FX A.S.L., E.C.S., R.E.H., J.F.C., and D.G.S. were supported by the Grant
Analysis of Titan's Interaction with Saturn's Magnetosphere using
Cassini Titan Flyby Data and Kinetic-Fluid Model from the NASA Cassini
Data Analysis Program (08-CDAP08-0043, PI - E.C. Sittler Jr.). A.S.L.
was also supported in part by the grants/tasks 900-37-172 and 670-90-315
between the GPHI UMBC and NASA GSFC. Computational resources
(supercomputers Endeavour and Pleiades (Ivy Bridge)) were provided by
the NASA Ames Advanced Supercomputing (NAS) Division (Projects
SMD-09-1124 and SMD-13-1517). The authors thank the referees for
fruitful comments.
NR 57
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U1 0
U2 3
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 APR
PY 2014
VL 93-94
BP 119
EP 128
DI 10.1016/j.pss.2014.02.012
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AG2WO
UT WOS:000335278000012
ER
PT J
AU Petch, J
Hill, A
Davies, L
Fridlind, A
Jakob, C
Lin, YL
Xie, SEC
Zhu, P
AF Petch, Jon
Hill, Adrian
Davies, Laura
Fridlind, Ann
Jakob, Christian
Lin, Yanluan
Xie, Shaoecheng
Zhu, Ping
TI Evaluation of intercomparisons of four different types of model
simulating TWP-ICE
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE convection; numerical modelling; microphysics
ID WEATHER PREDICTION; CLOUD; RAIN
AB Four model intercomparisons were run and evaluated using the TWP-ICE field campaign, each involving different types of atmospheric model. Here we highlight what can be learnt from having single-column model (SCM), cloud-resolving model (CRM), global atmosphere model (GAM) and limited-area model (LAM) intercomparisons all based around the same field campaign. We also make recommendations for anyone planning further large multi-model intercomparisons to ensure they are of maximum value to the model development community. CRMs tended to match observations better than other model types, although there were exceptions such as outgoing long-wave radiation. All SCMs grew large temperature and moisture biases and performed worse than other model types for many diagnostics. The GAMs produced a delayed and significantly reduced peak in domain-average rain rate when compared to the observations. While it was shown that this was in part due to the analysis used to drive these models, the LAMs were also driven by this analysis and did not have the problem to the same extent. Based on differences between the models with parametrized convection (SCMs and GAMs) and those without (CRMs and LAMs), we speculate that that having explicit convection helps to constrain liquid water whereas the ice contents are controlled more by the representation of the microphysics.
C1 [Petch, Jon; Hill, Adrian] Met Off, Exeter EX1 3PB, Devon, England.
[Davies, Laura] Univ Melbourne, Melbourne, Vic 3010, Australia.
[Fridlind, Ann] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Jakob, Christian] Monash Univ, Sch Math, Melbourne, Vic 3004, Australia.
[Lin, Yanluan] Tsinghua Univ, Ctr Earth Syst Sci, Beijing 100084, Peoples R China.
[Xie, Shaoecheng] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Zhu, Ping] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA.
RP Petch, J (reprint author), Met Off, FitzRoy Rd, Exeter EX1 3PB, Devon, England.
EM jon.petch@metoffice.gov.uk
RI lin, yanluan/A-6333-2015; Xie, Shaocheng/D-2207-2013; Jakob,
Christian/A-1082-2010
OI Xie, Shaocheng/0000-0001-8931-5145; Jakob, Christian/0000-0002-5012-3207
FU NASA Radiation Sciences Program; US DOE Office of Science, Office of
Biological and Environmental Research [DE-AI02-06ER64173, DE-SC0006712];
US Department of Energy (DOE), Office of Science, Office of Biological
and Environmental Research by Lawrence Livermore National Laboratory
[DE-AC52-07NA27344]; Atmospheric Radiation Measurement Program of the
Office of Science at the US Department of Energy; DOE ASR
[DE-FG02-09ER64737]; Office of Science (BER), US Department of Energy;
US DOE ASR program [DE-FG02-09ER64742]
FX A. Fridlind was supported by the NASA Radiation Sciences Program and the
US DOE Office of Science, Office of Biological and Environmental
Research, through contracts DE-AI02-06ER64173 and DE-SC0006712. The
contributions of S. Xie to this work were performed under the auspices
of the US Department of Energy (DOE), Office of Science, Office of
Biological and Environmental Research by Lawrence Livermore National
Laboratory under contract no. DE-AC52-07NA27344 and supported by the
Atmospheric Radiation Measurement Program of the Office of Science at
the US Department of Energy. Ping Zhu wishes to acknowledge his support
by the DOE ASR program under grant DE-FG02-09ER64737. Yanluan Lin was
supported by the Office of Science (BER), US Department of Energy. Laura
Davies and Christian Jakob were supported by the US DOE ASR program
under grant DE-FG02-09ER64742.
NR 19
TC 6
Z9 6
U1 0
U2 8
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2014
VL 140
IS 680
BP 826
EP 837
DI 10.1002/qj.2192
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF7WU
UT WOS:000334926800009
ER
PT J
AU Errico, RM
Prive, NC
AF Errico, Ronald M.
Prive, Nikki C.
TI An estimate of some analysis-error statistics using the Global Modeling
and Assimilation Office observing-system simulation framework
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE OSSE; atmospheric analysis; data assimilation; analysis error
ID VALIDATION
AB The observing-system simulation experiment (OSSE) framework developed at the National Aeronautics and Space Administration (NASA), Global Modeling and Assimilation Office (GMAO) is used to estimate some characteristics of analysis error. This is possible because, within the framework, the true state of the simulated atmosphere is known and, after suitable interpolation to a common grid, can be simply differenced with the analysis to compute errors explicitly. The only assumption is that the OSSE is sufficiently realistic so that error statistics derived from it adequately describe those obtained when analyzing observations of the real atmosphere. Attention here is restricted to the troposphere during the months of July and August at 0000 and 1200 UTC using an observation data set from 2011.
Analysis-error statistics presented here include geographical distributions of temporal variances, power spectra of spherical harmonics and correlations in meridional, latitudinal and vertical directions. Our most noteworthy results include the revelation through spectral analysis that only synoptic scales are well analyzed and that horizontal correlation lengths in the extratropics are short, with little vertical variation, and the dominance of rotational wind errors in contrast to divergent ones.
Also examined are fractional reductions in background-error variances due to analysis of observations. These reveal that in most geographical regions throughout the troposphere, errors are reduced by analyzing observations, as intended. The reductions are typically small, however (-10% in most regions), as should be expected from consideration of the equilibration of errors implied by the Kalman-filter equations.
C1 [Errico, Ronald M.; Prive, Nikki C.] Morgan State Univ, Goddard Earth Sci Technol & Res Ctr, Baltimore, MD 21239 USA.
[Errico, Ronald M.; Prive, Nikki C.] NASA, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Errico, RM (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA.
EM ronald.m.errico@nasa.gov
OI Prive, Nikki/0000-0001-8309-8741
FU GMAO
FX This OSSE was conducted with the assistance of Ricardo Todling, Meta
Sienkiewicz and Joseph Stassi at the GMAO. The ECMWF nature run was
provided by Erik Andersson through arrangements made by Michiko
Masutani. Support for this project was encouraged by Michele Rienecker
and provided by GMAO core funding.
NR 11
TC 7
Z9 7
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2014
VL 140
IS 680
BP 1005
EP 1012
DI 10.1002/qj.2180
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF7WU
UT WOS:000334926800024
ER
PT J
AU Coy, L
Reynolds, CA
AF Coy, Lawrence
Reynolds, Carolyn A.
TI Singular vectors and their nonlinear evolution during the January 2009
stratospheric sudden warming
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE stratosphere dynamics; sudden warming; singular vectors
ID ADAPTIVE OBSERVING GUIDANCE; ATLANTIC TROPICAL CYCLONES; TARGETED
OBSERVATIONS; PREDICTION SYSTEM; GROWTH; MODEL; FLOW; PREDICTABILITY;
PERTURBATIONS; CIRCULATION
AB The evolution and structure of stratospheric singular vectors (SVs) during the major stratospheric sudden warming (SSW) of January 2009 are investigated. SV analyses, optimized for growth at stratospheric levels over 72 h, were examined for selected dates before and during the SSW. It was found that the initial and final SV fields have larger horizontal structures during the SSW event than before the SSW event. A high-altitude forecast model was initialized with perturbations taken from the initial time SV structures and integrated for 144 h to study growth and nonlinear changes in a highly disturbed polar vortex. When large-amplitude initial SV perturbations were forecast during the SSW, large changes occurred in the descent of the SSW event and poleward focusing of the Eliassen-Palm fluxes. Examination of the development of SV analysis suggests that stratospheric SV growth occurs through wave-action conservation as initial SV perturbations propagate into the polar vortex jet.
C1 [Coy, Lawrence] Naval Res Lab, Washington, DC USA.
[Reynolds, Carolyn A.] Naval Res Lab, Monterey, CA USA.
RP Coy, L (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM lawrence.coy@nasa.gov
OI Reynolds, Carolyn/0000-0003-4690-4171
FU Office of Naval Research
FX This research was funded by the Office of Naval Research and performed
at the Naval Research Laboratory. Additional support was received via a
grant of computer time from the DOD High Performance Computing
Modernization Program.
NR 39
TC 0
Z9 0
U1 1
U2 8
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2014
VL 140
IS 680
BP 1013
EP 1024
DI 10.1002/qj.2181
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AF7WU
UT WOS:000334926800025
ER
PT J
AU Rochdane, S
Bounoua, L
Zhang, P
Imhoff, ML
Messouli, M
Yacoubi-Khebiza, M
AF Rochdane, Saloua
Bounoua, Lahouari
Zhang, Ping
Imhoff, Marc L.
Messouli, Mohammed
Yacoubi-Khebiza, Mohammed
TI Combining Satellite Data and Models to Assess Vulnerability to Climate
Change and Its Impact on Food Security in Morocco
SO SUSTAINABILITY
LA English
DT Article
DE satellite; model; vulnerability index; climate change; food security;
Morocco
ID NET PRIMARY PRODUCTION; MODIS; ADAPTATION; VEGETATION
AB This work analyzes satellite and socioeconomic data to explore the relationship between food and wood demand and supply, expressed in terms of net primary production (NPP), in Morocco. A vulnerability index is defined as the ratio of demand to supply as influenced by population, affluence, technology and climate indicators. The present situation (1995-2007), as well as projections of demand and supply, following the Intergovernmental Panel on Climate Change, Scenarios A2 and B2, are analyzed for a 2025 horizon. We find that the food NPP demand increased by 34.5%, whereas the wood consumption NPP demand decreased by 19.3% between 1995 and 2007. The annual NPP required to support the population's food and wood appropriation was 29.73 million tons of carbon (MTC) in 2007, while the landscape NPP production for the same year was 60.24 MTC; indicating that the population appropriates about 50% of the total NPP resources. Both scenarios show increases in demand and decreases in supply. Under A2, it would take more than 1.25 years for terrestrial ecosystems in Morocco to produce the NPP appropriated by populations in one year. This number is 0.70 years under B2. This already high vulnerability for food and wood products is likely to be exacerbated with climate changes and population increase.
C1 [Rochdane, Saloua; Messouli, Mohammed; Yacoubi-Khebiza, Mohammed] Cadi Ayyad Univ, Fac Sci Semlalia, Dept Environm Sci, Marrakech 40000, Morocco.
[Bounoua, Lahouari; Zhang, Ping] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zhang, Ping] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Imhoff, Marc L.] Joint Global Change Res Inst 5825 Univ Res Court, College Pk, MD 20742 USA.
RP Bounoua, L (reprint author), NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Code 618, Greenbelt, MD 20771 USA.
EM rochdane@yahoo.fr; lahouari.bounoua@nasa.gov; ping.zhang@nasa.gov;
Marc.Imhoff@pnnl.gov; messouli@ucam.ac.ma; yacoubi@ucam.ac.ma
FU African Climate Change Fellowship Program (ACCFP); System for Analysis
Research and Training (START) secretariat
FX The authors would like to thank the African Climate Change Fellowship
Program (ACCFP) and the System for Analysis Research and Training
(START) secretariat for their financial support. Thanks are also
extended to the staff of the Biospheric Sciences Laboratory of NASA's
Goddard Space Flight Center.
NR 36
TC 2
Z9 2
U1 3
U2 22
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2071-1050
J9 SUSTAINABILITY-BASEL
JI Sustainability
PD APR
PY 2014
VL 6
IS 4
BP 1729
EP 1746
DI 10.3390/su6041729
PG 18
WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Environmental Sciences;
Environmental Studies
SC Science & Technology - Other Topics; Environmental Sciences & Ecology
GA AF7VA
UT WOS:000334921800006
ER
PT J
AU Ade, PAR
Aghanim, N
Alves, MIR
Arnaud, M
Ashdown, M
Atrio-Barandela, F
Aumont, J
Baccigalupi, C
Banday, AJ
Barreiro, RB
Bartlett, JG
Battaner, E
Benabed, K
Benoit-Levy, A
Bernard, JP
Bersanelli, M
Bielewicz, P
Bobin, J
Bonaldi, A
Bond, JR
Borrill, J
Bouchet, FR
Boulanger, F
Bucher, M
Burigana, C
Butler, RC
Cardoso, JF
Catalano, A
Chamballu, A
Chiang, HC
Chiang, LY
Christensen, PR
Clements, DL
Colombi, S
Colombo, LPL
Couchot, F
Crill, BP
Curto, A
Cuttaia, F
Danese, L
Davies, RD
Davis, RJ
de Bernardis, P
de Rosa, A
de Zotti, G
Delabrouille, J
Dickinson, C
Diego, JM
Dole, H
Donzelli, S
Dore, O
Douspis, M
Dupac, X
Ensslin, TA
Eriksen, HK
Falgarone, E
Finelli, F
Forni, O
Frailis, M
Franceschi, E
Galeotta, S
Ganga, K
Ghosh, T
Giard, M
Giardino, G
Gonzalez-Nuevo, J
Gorski, KM
Gregorio, A
Gruppuso, A
Hansen, FK
Harrison, D
Hernandez-Monteagudo, C
Herranz, D
Hildebrandt, SR
Hivon, E
Holmes, WA
Hornstrup, A
Hovest, W
Jaffe, AH
Jones, WC
Juvela, M
Keihanen, E
Keskitalo, R
Kisner, TS
Kneissl, R
Knoche, J
Kunz, M
Kurki-Suonio, H
Lagache, G
Lahteenmaki, A
Lamarre, JM
Lasenby, A
Laureijs, RJ
Lawrence, CR
Leonardi, R
Levrier, F
Liguori, M
Lilje, PB
Linden-Vornle, M
Lopez-Caniego, M
Macias-Perez, JF
Maffei, B
Maino, D
Mandolesi, N
Maris, M
Marshall, DJ
Martin, PG
Martinez-Gonzalez, E
Masi, S
Matarrese, S
Mazzotta, P
Melchiorri, A
Mendes, L
Mennella, A
Migliaccio, M
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
Oxborrow, CA
Pagano, L
Pajot, F
Paladini, R
Paoletti, D
Pasian, F
Patanchon, G
Peel, M
Perdereau, O
Perrotta, F
Piacentini, F
Piat, M
Pierpaoli, E
Pietrobon, D
Plaszczynski, S
Pointecouteau, E
Polenta, G
Ponthieu, N
Popa, L
Pratt, GW
Prunet, S
Puget, JL
Rachen, JP
Reach, WT
Rebolo, R
Reinecke, M
Remazeilles, M
Renault, C
Ricciardi, S
Riller, T
Ristorcelli, I
Rocha, G
Rosset, C
Rubino-Martin, JA
Rusholme, B
Sandri, M
Savini, G
Scott, D
Spencer, LD
Starck, JL
Stolyarov, V
Sureau, F
Sutton, D
Suur-Uski, AS
Sygnet, JF
Tauber, JA
Tavagnacco, D
Terenzi, L
Toffolatti, L
Tomasi, M
Tristram, M
Tucci, M
Valenziano, L
Valiviita, J
Van Tent, B
Verstraete, L
Vielva, P
Villa, F
Vittorio, N
Wade, LA
Wandelt, BD
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.
Banday, A. J.
Barreiro, R. B.
Bartlett, J. G.
Battaner, E.
Benabed, K.
Benoit-Levy, A.
Bernard, J. -P.
Bersanelli, M.
Bielewicz, P.
Bobin, J.
Bonaldi, A.
Bond, J. R.
Borrill, J.
Bouchet, F. R.
Boulanger, F.
Bucher, M.
Burigana, C.
Butler, R. C.
Cardoso, J. -F.
Catalano, A.
Chamballu, A.
Chiang, H. C.
Chiang, L. -Y.
Christensen, P. R.
Clements, D. L.
Colombi, S.
Colombo, L. P. L.
Couchot, F.
Crill, B. P.
Curto, A.
Cuttaia, F.
Danese, L.
Davies, R. D.
Davis, R. J.
de Bernardis, P.
de Rosa, A.
de Zotti, G.
Delabrouille, J.
Dickinson, C.
Diego, J. M.
Dole, H.
Donzelli, S.
Dore, O.
Douspis, M.
Dupac, X.
Ensslin, T. A.
Eriksen, H. K.
Falgarone, E.
Finelli, F.
Forni, O.
Frailis, M.
Franceschi, E.
Galeotta, S.
Ganga, K.
Ghosh, T.
Giard, M.
Giardino, G.
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.
Holmes, W. A.
Hornstrup, A.
Hovest, W.
Jaffe, A. H.
Jones, W. C.
Juvela, M.
Keihanen, E.
Keskitalo, R.
Kisner, T. S.
Kneissl, R.
Knoche, J.
Kunz, M.
Kurki-Suonio, H.
Lagache, G.
Lahteenmaki, A.
Lamarre, J. -M.
Lasenby, A.
Laureijs, R. J.
Lawrence, C. R.
Leonardi, R.
Levrier, F.
Liguori, M.
Lilje, P. B.
Linden-Vornle, M.
Lopez-Caniego, M.
Macias-Perez, J. F.
Maffei, B.
Maino, D.
Mandolesi, N.
Maris, M.
Marshall, D. J.
Martin, P. G.
Martinez-Gonzalez, E.
Masi, S.
Matarrese, S.
Mazzotta, P.
Melchiorri, A.
Mendes, L.
Mennella, A.
Migliaccio, M.
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.
Oxborrow, C. A.
Pagano, L.
Pajot, F.
Paladini, R.
Paoletti, D.
Pasian, F.
Patanchon, G.
Peel, M.
Perdereau, O.
Perrotta, F.
Piacentini, F.
Piat, M.
Pierpaoli, E.
Pietrobon, D.
Plaszczynski, S.
Pointecouteau, E.
Polenta, G.
Ponthieu, N.
Popa, L.
Pratt, G. W.
Prunet, S.
Puget, J. -L.
Rachen, J. P.
Reach, W. T.
Rebolo, R.
Reinecke, M.
Remazeilles, M.
Renault, C.
Ricciardi, S.
Riller, T.
Ristorcelli, I.
Rocha, G.
Rosset, C.
Rubino-Martin, J. A.
Rusholme, B.
Sandri, M.
Savini, G.
Scott, D.
Spencer, L. D.
Starck, J. -L.
Stolyarov, V.
Sureau, F.
Sutton, D.
Suur-Uski, A. -S.
Sygnet, J. -F.
Tauber, J. A.
Tavagnacco, D.
Terenzi, L.
Toffolatti, L.
Tomasi, M.
Tristram, M.
Tucci, M.
Valenziano, L.
Valiviita, J.
Van Tent, B.
Verstraete, L.
Vielva, P.
Villa, F.
Vittorio, N.
Wade, L. A.
Wandelt, B. D.
Yvon, D.
Zacchei, A.
Zonca, A.
CA Planck Collaboration
TI Planck intermediate results. XIV. Dust emission at millimetre
wavelengths in the Galactic plane
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: general; Galaxy: general; radiation mechanisms: general; radio
continuum: ISM; submillimeter: ISM
ID PRE-LAUNCH STATUS; SPECTRAL ENERGY-DISTRIBUTIONS; MU-M; MAGNETIC
NANOPARTICLES; TEMPERATURE-DEPENDENCE; SUBMILLIMETER EXCESS; MICROWAVE
EMISSION; INTERSTELLAR DUST; MAGELLANIC CLOUDS; MOLECULAR CLOUDS
AB We use Planck HFI data combined with ancillary radio data to study the emissivity index of the interstellar dust emission in the frequency range 100-353 GHz, or 3-0.8 mm, in the Galactic plane. We analyse the region l = 20 degrees-44 degrees and vertical bar b vertical bar <= 4 degrees where the free-free emission can be estimated from radio recombination line data. We fit the spectra at each sky pixel with a modified blackbody model and two opacity spectral indices, beta(mm) and beta(FIR), below and above 353 GHz, respectively. We find that beta(mm) is smaller than beta(FIR), and we detect a correlation between this low frequency power-law index and the dust optical depth at 353 GHz, tau(353). The opacity spectral index beta(mm) increases from about 1.54 in the more diffuse regions of the Galactic disk, vertical bar b vertical bar = 3 degrees-4 degrees and tau(353) similar to 5 x 10(-5), to about 1.66 in the densest regions with an optical depth of more than one order of magnitude higher. We associate this correlation with an evolution of the dust emissivity related to the fraction of molecular gas along the line of sight. This translates into beta(mm) similar to 1.54 for a medium that is mostly atomic and beta(mm) similar to 1.66 when the medium is dominated by molecular gas. We find that both the two-level system model and magnetic dipole emission by ferromagnetic particles can explain the results. These results improve our understanding of the physics of interstellar dust and lead towards a complete model of the dust spectrum of the Milky Way from far-infrared to millimetre wavelengths.
C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, Observ Paris,Sorbonne Paris Cite,APC, F-75205 Paris 13, France.
[Lahteenmaki, A.] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland.
[Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, Aalto 00076, Finland.
[Kunz, M.] African Inst Math Sci, ZA-7701 Rondebosch, South Africa.
[Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy.
[Mandolesi, N.] Agenzia Spaziale Italiana, I-00198 Rome, Italy.
[Ashdown, M.; Curto, A.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
[Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa.
[Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Santiago 0355, Chile.
[Bond, J. R.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Crill, B. P.; Dore, O.; Hildebrandt, S. R.; Rocha, G.; Savini, G.] CALTECH, Pasadena, CA 91125 USA.
[Hernandez-Monteagudo, C.] Ctr Estudios Fis Cosmos Aragon, 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 28037, Spain.
[Chamballu, A.; 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.
[Kunz, M.; Tucci, 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, Dept Astrophys, IMAPP, 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.
[Benoit-Levy, A.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Chiang, H. C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA.
[Liguori, M.; 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.; Pagano, L.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Bersanelli, M.; Maino, D.; Mennella, A.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy.
[Gregorio, A.; Tavagnacco, D.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, 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, E-38206 Tenerife, Spain.
[Kneissl, R.] ESO Vitacura, European So Observ, Santiago 19001, Chile.
[Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain.
[Giardino, G.; Laureijs, R. J.; Tauber, J. A.] Estec, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands.
[Kurki-Suonio, H.; Lahteenmaki, A.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland.
[de Zotti, G.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[Polenta, G.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Frailis, M.; Galeotta, S.; Gregorio, A.; Maris, M.; Pasian, F.; Tavagnacco, D.; Zacchei, A.] INAF Osservatorio Astron Trieste, I-34143 Trieste, 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.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASE Bologna, I-40129 Bologna, Italy.
[Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Tomasi, M.] INAF IASF Milano, I-20133 Milan, Italy.
[Finelli, F.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy.
[Melchiorri, A.; Pagano, L.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy.
[Gregorio, A.] Natl Inst Nucl Phys, I-34127 Trieste, Italy.
[Ponthieu, N.] Univ Grenoble 1, CNRS INSU, UMR 5274, Inst Planetol & Astrophys Grenoble, F-38041 Grenoble, France.
[Mitra, S.] IUCAA, Pune 411007, Maharashtra, India.
[Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Paladini, R.; Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Dole, H.] Inst Univ France, F-75005 Paris, France.
[Aghanim, N.; Alves, M. I. R.; Aumont, J.; Boulanger, F.; Chamballu, A.; Dole, H.; Douspis, M.; Ghosh, T.; Kunz, M.; Lagache, G.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Remazeilles, M.; Verstraete, L.] Univ Paris 11, UMR8617, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France.
[Popa, L.] Inst Space Sci, Bucharest 077125, Romania.
[Chiang, L. -Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Harrison, D.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife 38205, Spain.
[Barreiro, R. B.; Curto, A.; 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.; Colombo, L. P. L.; Crill, B. P.; 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.; Remazeilles, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Ashdown, M.; Harrison, D.; Lasenby, A.; Migliaccio, M.; Stolyarov, V.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
[Couchot, F.; Perdereau, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, CNRS, IN2P3, LAL, F-91405 Orsay, France.
[Catalano, A.; Falgarone, E.; Lamarre, J. -M.; Levrier, F.] CNRS, Observ Paris, LERMA, F-75014 Paris, France.
[Arnaud, M.; Bobin, J.; Chamballu, A.; Marshall, D. J.; Pratt, G. W.; Starck, J. -L.; Sureau, F.] Univ Paris Diderot, CEA DSM CNRS, Serv Astrophys, Lab AIM,IRFU, 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.
[Catalano, A.; Macias-Perez, J. F.; Renault, C.] Univ Grenoble 1, CNRS IN2P3, Inst Natl Polytech Grenoble, Lab Phys Subatom & Cosmol, 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.; Riller, T.] Max Planck Inst Astrophys, D-85741 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.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Ade, P. A. R.; Munshi, D.; Spencer, L. D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales.
[Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Zelenchukskiy Region, Karachai Cherke, Russia.
[Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR7095, F-75014 Paris, France.
[Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; 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.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Alves, MIR (reprint author), Univ Paris 11, UMR8617, CNRS, Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France.
EM marta.alves@ias.u-psud.fr
RI Butler, Reginald/N-4647-2015; Remazeilles, Mathieu/N-1793-2015;
Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016;
Kurki-Suonio, Hannu/B-8502-2016; 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; Lahteenmaki,
Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Herranz,
Diego/K-9143-2014; Lopez-Caniego, Marcos/M-4695-2013; Bobin,
Jerome/P-3729-2014; Battaner, Eduardo/P-7019-2014; Vielva,
Patricio/F-6745-2014; 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
OI Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego,
Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta,
Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996;
Cuttaia, Francesco/0000-0001-6608-5017; Burigana,
Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924;
Pierpaoli, Elena/0000-0002-7957-8993; Zacchei,
Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje,
Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini,
Giorgio/0000-0003-4449-9416; 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; Reach, William/0000-0001-8362-4094; Peel,
Mike/0000-0003-3412-2586; Scott, Douglas/0000-0002-6878-9840; Masi,
Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446;
Remazeilles, Mathieu/0000-0001-9126-6266; Maris,
Michele/0000-0001-9442-2754; Galeotta, Samuele/0000-0002-3748-5115;
Pasian, Fabio/0000-0002-4869-3227; WANDELT,
Benjamin/0000-0002-5854-8269; Rubino-Martin, Jose
Alberto/0000-0001-5289-3021; Finelli, Fabio/0000-0002-6694-3269; De
Zotti, Gianfranco/0000-0003-2868-2595; Sandri,
Maura/0000-0003-4806-5375; Franceschi, Enrico/0000-0002-0585-6591;
Valenziano, Luca/0000-0002-1170-0104; Morgante,
Gianluca/0000-0001-9234-7412; Matarrese, Sabino/0000-0002-2573-1243;
Valiviita, Jussi/0000-0001-6225-3693; Mazzotta,
Pasquale/0000-0002-5411-1748; 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;
Toffolatti, Luigi/0000-0003-2645-7386; Herranz,
Diego/0000-0003-4540-1417; Bobin, Jerome/0000-0003-1457-7890; Vielva,
Patricio/0000-0003-0051-272X; 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;
FU ESA (France); CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy);
CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK);
CSIC (Spain); MICINN (Spain); JA (Spain); Tekes (Finland); AoF
(Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada);
DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland);
FCT/MCTES (Portugal); DEISA (EU); European Research Council under the
European Union [267934]
FX We acknowledge the use of the HEALPix (Gorski et al. 2005) package and
IRAS data. The Planck Collaboration acknowledges support from: 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 DEISA (EU). A detailed description of the Planck
Collaboration and a list of its members can be found at
http://www.rssd.esa.int/index.php?project=PLANCK&page-Planck-Collaborati
on. The research leading to these results has received funding from the
European Research Council under the European Union's Seventh Framework
Programme (FP7/2007-2013)/ERC grant agreement no 267934.
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PD APR
PY 2014
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF4GW
UT WOS:000334671000045
ER
PT J
AU Beck, PG
Hambleton, K
Vos, J
Kallinger, T
Bloemen, S
Tkachenko, A
Garcia, RA
Ostensen, RH
Aerts, C
Kurtz, DW
De Ridder, J
Hekker, S
Pavlovski, K
Mathur, S
De Smedt, K
Derekas, A
Corsaro, E
Mosser, B
Van Winckel, H
Huber, D
Degroote, P
Davies, GR
Prsa, A
Debosscher, J
Elsworth, Y
Nemeth, P
Siess, L
Schmid, VS
Papics, PI
de Vries, BL
van Marle, AJ
Marcos-Arenal, P
Lobel, A
AF Beck, P. G.
Hambleton, K.
Vos, J.
Kallinger, T.
Bloemen, S.
Tkachenko, A.
Garcia, R. A.
Ostensen, R. H.
Aerts, C.
Kurtz, D. W.
De Ridder, J.
Hekker, S.
Pavlovski, K.
Mathur, S.
De Smedt, K.
Derekas, A.
Corsaro, E.
Mosser, B.
Van Winckel, H.
Huber, D.
Degroote, P.
Davies, G. R.
Prsa, A.
Debosscher, J.
Elsworth, Y.
Nemeth, P.
Siess, L.
Schmid, V. S.
Papics, P. I.
de Vries, B. L.
van Marle, A. J.
Marcos-Arenal, P.
Lobel, A.
TI Pulsating red giant stars in eccentric binary systems discovered from
Kepler space-based photometry A sample study and the analysis of KIC
5006817
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: solar-type; binaries: general; stars: rotation; Sun:
oscillations; stars: individual: KIC5006817; asteroseismology
ID SOLAR-LIKE OSCILLATIONS; SUBDWARF-B-STARS; STELLAR ASTROPHYSICS MESA;
ECLIPSING BINARY; LIGHT CURVES; FORMATION CHANNELS; SCALING RELATIONS;
EQUILIBRIUM TIDE; VELOCITY CURVES; MAIN-SEQUENCE
AB Context. The unparalleled photometric data obtained by NASA's Kepler Space Telescope has led to improved understanding of red giant stars and binary stars. Seismology allows us to constrain the properties of red giants. In addition to eclipsing binaries, eccentric non-eclipsing binaries that exhibit ellipsoidal modulations have been detected with Kepler.
Aims. We aim to study the properties of eccentric binary systems containing a red giant star and to derive the parameters of the primary giant component.
Methods. We applied asteroseismic techniques to determine the masses and radii of the primary component of each system. For a selected target, light and radial velocity curve modelling techniques were applied to extract the parameters of the system and its primary component. Stellar evolution and its effects on the evolution of the binary system were studied from theoretical models.
Results. The paper presents the asteroseismic analysis of 18 pulsating red giants in eccentric binary systems, for which masses and radii were constrained. The orbital periods of these systems range from 20 to 440 days. The results of our ongoing radial velocity monitoring progranune with the Hermes spectrograph reveal an eccentricity range of e = 0.2 to 0.76. As a case study we present a detailed analysis of KIC 5006817, whose rich oscillation spectrum allows for detailed seismic analysis. From seismology we constrain the rotational period of the envelope to be at least 165 d, which is roughly twice the orbital period. The stellar core rotates 13 times faster than the surface. From the spectrum and radial velocities we expect that the Doppler beaming signal should have a maximum amplitude of 300 ppm in the light curve. Fixing the mass and radius to the asteroseismically determined values, we find from our binary modelling a value of the gravity darkening exponent that is significantly larger than expected. Through binary modelling, we determine the mass of the secondary component to be 0.29 +/- 0.03 M circle dot.
Conclusions. For KIC 5006817 we exclude pseudo-synchronous rotation of the red giant with the orbit. The comparison of the results from seismology and modelling of the light curse shows a possible alignment of the rotational and orbital axis at the 2 sigma level. Red giant eccentric systems could be progenitors of cataclysmic variables and hot subdwarf B stars.
C1 [Beck, P. G.; Hambleton, K.; Vos, J.; Bloemen, S.; Tkachenko, A.; Ostensen, R. H.; Aerts, C.; De Ridder, J.; De Smedt, K.; Corsaro, E.; Van Winckel, H.; Degroote, P.; Debosscher, J.; Nemeth, P.; Schmid, V. S.; Papics, P. I.; de Vries, B. L.; van Marle, A. J.; Marcos-Arenal, P.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium.
[Hambleton, K.; Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Kallinger, T.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Garcia, R. A.] Univ Paris 07, IRFU SAp, CEA DSM CNRS, Lab AIM, F-91191 Gif Sur Yvette, France.
[Aerts, C.] Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
[Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Pavlovski, K.] Univ Zagreb, Fac Sci, Dept Phys, Zagreb 10000, Croatia.
[Mathur, S.] Space Sci Inst, Boulder, CO 80301 USA.
[Derekas, A.] Hungarian Acad Sci, Res Ctr F Astron & Earth Sci, Konkoly Observ, H-1121 Budapest, Hungary.
[Mosser, B.] Univ Paris 07, Observ Paris, Univ Paris 06, LESIA,CNRS, F-92195 Meudon, France.
[Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Davies, G. R.; Elsworth, Y.] Univ Birmingham, Sch Phys & Astron, Birmingham B13 2TT, W Midlands, England.
[Prsa, A.] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
[Siess, L.] Univ Libre Bruxelles, Inst Astron & Astrophys, B-1050 Brussels, Belgium.
[Lobel, A.] Royal Observ Belgium, B-1180 Brussels, Belgium.
RP Beck, PG (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium.
EM paul.beck@ster.kuleuven.be
RI Nemeth, Peter/E-4515-2016; Derekas, Aliz/G-2091-2016; Marcos-Arenal,
Pablo/O-4719-2016;
OI Davies, Guy/0000-0002-4290-7351; Nemeth, Peter/0000-0003-0963-0239;
Derekas, Aliz/0000-0002-6526-9444; Marcos-Arenal,
Pablo/0000-0003-1549-9396; Kallinger, Thomas/0000-0003-3627-2561;
Garcia, Rafael/0000-0002-8854-3776
FU NASA's Science Mission Directorate; NASA [NNX12AE17G]; Research Council
of the KU Leuven [GOA/2013/012]; European Research Council under the
European Community [227224]; European Community [312844]; UK STFC PhD
grant; EWO-Handers [06260-G.0728.11]; Austrian Science Fund [FWF
P23608]; Fund for Scientific Research; Netherlands Organisation for
Scientific Research (NWO); Aspirant Ph.D. Fellow of the FWO, Belgium;
Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences;
Hungarian OTKA [K76816, K83790, MBO8C 81013, KTIA URKUT_10 1 2011-0019];
Hungarian Academy of Sciences
FX We acknowledge the work of the team behind Kepler. Funding for the
Kepler Mission is provided by NASA's Science Mission Directorate. The
ground-based follow-up observations are based on spectroscopy made with
the Mercator Telescope, operated on the island of La Palma by the
Flemish Community, at the Spanish Observatorio del Roque de los
Muchachos of the Instituto de Astrofisica de Canarias. This work
partially used data analyzed under the NASA grant NNX12AE17G. This
research is (partially) funded by the Research Council of the KU Leuven
under grant agreement GOA/2013/012. The research leading to these
results has received funding from the European Research Council under
the European Community's Seventh Framework Programme FP7/2007-2013)/ERC
grant agreement no 227224 (PROSPERITY). The research leading to these
results has received funding 'from the European Community's Seventh
Framework Programme FP7-SPACE-2011-1 , project number 312844 (SPACEINN).
K.H. was supported by a UK STFC PhD grant. J.D.R., T.K. and E.C.
acknowledge the support of the EWO-Handers wider project 06260-
G.0728.11. T.K. also acknowledges financial support from the Austrian
Science Fund (FWF P23608). A.T. was supported by the Fund for Scientific
Research. S.H. was supported by the Netherlands Organisation for
Scientific Research (NWO). V.S.S. is an Aspirant Ph.D. Fellow of the
FWO, Belgium. A.D. is supported by a Janos Bolyai Research Scholarship
of the Hungarian Academy of Sciences. This project has been supported by
the Hungarian OTKA Grants K76816, K83790, MBO8C 81013 and KTIA URKUT_10
1 2011-0019 grant and the "Lendulet2009" Young Researchers Programme of
the Hungarian Academy of Sciences. P.G.B thanks Nick Cox for
observational work.
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JI Astron. Astrophys.
PD APR
PY 2014
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DI 10.1051/0004-6361/201322477
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF4GW
UT WOS:000334671000036
ER
PT J
AU Deleuil, M
Almenara, JM
Santerne, A
Barros, SCC
Havel, M
Hebrard, G
Bonomo, AS
Bouchy, F
Bruno, U
Damiani, C
Diaz, RF
Montagnier, U
Moutou, C
AF Deleuil, M.
Almenara, J. -M.
Santerne, A.
Barros, S. C. C.
Havel, M.
Hebrard, G.
Bonomo, A. S.
Bouchy, F.
Bruno, U.
Damiani, C.
Diaz, R. F.
Montagnier, U.
Moutou, C.
TI SOPHIE velocimetry of Kepler transit candidates XI. Kepler-412 system:
probing the properties of a new inflated hot Jupiter
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planetary systems; techniques: photometric; techniques: radial
velocities; stars: fundamental parameters
ID COROT SPACE MISSION; EXTRASOLAR PLANETS; GIANT PLANET; LIGHT CURVES;
ATMOSPHERIC CHARACTERIZATION; SECONDARY ECLIPSE; DWARF COMPANION; HIGH
ALBEDO; MASS STARS; EXOPLANETS
AB Context. Hot Jupiters are still a fascinating exoplanet population that presents a diversity we are still far from understanding. High-precision photometric observations combined with radial velocity measurements give us a unique opportunity to constrain their properties better, on both their internal structure and their atmospheric bulk properties.
Aims. We initiated a follow-up program of Kepler-released planet candidates with the goal of confirming the planetary nature of a number of them through radial velocity measurements. For those that successfully passed the radial velocity screening, we furthermore performed a detailed exploration of their properties to characterize the systems. As a byproduct, these systematic observations allow us to consolidate the exoplanets' occurrence rate.
Methods. We performed a complete analysis of the Kepler-412 system, listed as planet candidate KOI-202 in the Kepler catalog, by combining the Kepler observations from Q1 to Q15, to ground-based spectroscopic observations that allowed us to derive radial velocity measurements, together with the host-star parameters and properties. We also analyzed the light curve to derive the star's rotation period and the phase function of the planet, including the secondary eclipse.
Results. We secured the planetary nature of Kepler-412b. We found the planet has a mass of 0.939 +/- 0.085 M-Jup and a radius of 1.325 +/- 0.043 R-Jup, which makes it a member of the bloated giant subgroup. It orbits its G3 V host star in 1.72 days. The system has an isochronal age of 5.1 Gyr, consistent with its moderate stellar activity as observed in the Kepler light curve and the rotation of the star of 17.2 +/- 1.6 days. From the detected secondary we derived the day-side temperature as a function of the geometric albedo. We estimated that the geometrical albedo A(g), should be between 0.094 +/- 0.015 and 0.013 (+0.017)(-0.013) and the brightness of the day side 2380 +/- 40 K. The measured night-side flux corresponds to a night-side brightness temperature of 2154 +/- 83 K, much greater than what is expected for a planet with homogeneous heat redistribution. From the comparison to star and planet evolution models, we found that dissipation should operate in the deep interior of the planet. This modeling also shows that despite its inflated radius, the planet presents a noticeable amount of heavy elements, which accounts for a mass fraction of 0.11 +/- 0.04.
C1 [Deleuil, M.; Almenara, J. -M.; Santerne, A.; Barros, S. C. C.; Bouchy, F.; Bruno, U.; Damiani, C.; Diaz, R. F.; Moutou, C.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France.
[Santerne, A.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Havel, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hebrard, G.; Montagnier, U.] Observ Haute Provence, F-04670 St Michel Lobservatoire, France.
[Hebrard, G.; Montagnier, U.] Inst Astrophys Paris, F-75014 Paris, France.
[Bonomo, A. S.] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, Italy.
RP Deleuil, M (reprint author), Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France.
EM magali.deleuil@lam.fr
OI Barros, Susana/0000-0003-2434-3625; Santerne,
Alexandre/0000-0002-3586-1316; Diaz, Rodrigo/0000-0001-9289-5160
FU PNP of CNRS/INSU; French ANR; CNES via postdoctoral fellowship program;
European Research Council/European Community under the FP7 [239953];
NASA Postdoctoral Program at the Ames Research Center; INAF/HARPS-N
fellowship; [98761]; [251091]; [426808]
FX This work is based on observations collected with the NASA's satellite
Kepler, the SOPHIE spectrograph on the 1.93-m telescope at the
Observatoire de Haute-Provence (CNRS), France. The authors thank the
staff at the Haute-Provence Observatory. They also acknowledge the PNP
of CNRS/INSU and the French ANR for their support. The team at LAM
acknowledges support by grants 98761 (SCCB), 251091 (JMA), and 426808
(CD). R.F.D. was supported by the CNES via its postdoctoral fellowship
program. A.S. acknowledges support from the European Research
Council/European Community under the FP7 through Starting Grant
agreement number 239953. M.H. was supported by an appointment to the
NASA Postdoctoral Program at the Ames Research Center, administered by
Oak Ridge Associated Universities through a contract with NASA. ASB
gratefully acknowledges support through INAF/HARPS-N fellowship.
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SC Astronomy & Astrophysics
GA AF4GW
UT WOS:000334671000056
ER
PT J
AU Guarrasi, M
Reale, E
Orlando, S
Mignone, A
Klimchuk, JA
AF Guarrasi, M.
Reale, E.
Orlando, S.
Mignone, A.
Klimchuk, J. A.
TI MHD modeling of coronal loops: the transition region throat
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: corona; Sun: magnetic fields; Sun: transition region;
magnetohydrodynamics (MHD)
ID SOLAR CORONA; THERMAL CONDUCTION; RADIATIVE LOSSES; ATOMIC DATABASE;
MAGNETIC-FIELD; EMISSION-LINES; SIMULATIONS; DYNAMICS; CORE; ABUNDANCES
AB Context. The expansion of coronal loops in the transition region may considerably influence the diagnostics of the plasma emission measure. The cross-sectional area of the loops is expected to depend on the temperature and pressure, and might be sensitive to the heating rate.
Aims. The approach here is to study the area response to slow changes in the coronal heating rate, and check the current interpretation in terms of steady heating models.
Methods. We study the area response with a time-dependent 2D magnetohydrodynamic (MHD) loop model, including the description of the expanding magnetic field, coronal heating and losses by thermal conduction, and radiation from optically thin plasma. We run a simulation for a loop 50 Mm long and quasi-statically heated to about 4 MK.
Results. We find that the area can change substantially with the quasi-steady heating rate, e.g., by similar to 40% at 0.5 MK as the loop temperature varies between 1 MK and 4 MK, and, therefore, affects the interpretation of the differential emission measure vs. temperature (DEM(T)) curves.
C1 [Guarrasi, M.; Reale, E.] Univ Palermo, Dipartimento Fis & Chim, I-90134 Palermo, Italy.
[Reale, E.; Orlando, S.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy.
[Mignone, A.] Univ Turin, Dipartimento Fis Gen, I-10125 Turin, Italy.
[Klimchuk, J. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Guarrasi, M (reprint author), Univ Palermo, Dipartimento Fis & Chim, Piazza Parlamento 1, I-90134 Palermo, Italy.
EM m.guarrasi@cineca.it
RI Klimchuk, James/D-1041-2012;
OI Klimchuk, James/0000-0003-2255-0305; Orlando,
Salvatore/0000-0003-2836-540X; Reale, Fabio/0000-0002-1820-4824
FU Italian Minister dell'Universita e Ricerca; Agenzia Spaziale Italiana
(ASI) [I/023/09/0, I/015/07/0]; CINECA under the ISCRA initiative
[HP10CWS0PW, HP10B54VL7]; HPC facility (SCAN) of the INAF - Osservatorio
Astronomico di Palermo; NASA
FX We thank the anonymous referee for constructive comments and
suggestions. We acknowledge support from the Italian Minister
dell'Universita e Ricerca and Agenzia Spaziale Italiana (ASI), contract
I/023/09/0 and I/015/07/0. PLUTO was developed at the Astronomical
Observatory of Turin in collaboration with the Department of Physics at
the University of Turin. We acknowledge the CINECA awards no. HP10CWS0PW
and no. HP10B54VL7 under the ISCRA initiative, and the HPC facility
(SCAN) of the INAF - Osservatorio Astronomico di Palermo, for the
availability of high-performance computing resources and support.
CHIANTI is a collaborative project involving the NRL (USA), the
Universities of Florence (Italy) and Cambridge (UK), and George Mason
University (USA). The work of J.A.K. was supported by the NASA
Supporting Research and Technology Program. We thank the International
Space Science Institute (ISSI) for hosting the International Team of S.
Bradshaw and H. Mason: Coronal Heating - Using Observables to Settle the
Question of Steady vs. Impulsive Heating.
NR 33
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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 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2014
VL 564
AR A48
DI 10.1051/0004-6361/201322848
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF4GW
UT WOS:000334671000048
ER
PT J
AU Langer, WD
Pineda, JL
Velusamy, T
AF Langer, W. D.
Pineda, J. L.
Velusamy, T.
TI The scale height of gas traced by [C II] in the Galactic plane
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: structure; ISM: clouds; ISM: atoms; infrared: ISM
ID MILKY-WAY; MOLECULAR CLOUDS; COLLISIONAL EXCITATION; HI DISTRIBUTION;
GALAXY; EMISSION; EQUILIBRIUM; PRESSURE; DISK; COBE
AB Context. The distribution of various interstellar gas components and the pressure in the interstellar medium (ISM) is a result of the interplay of different dynamical mechanisms and energy sources on the gas in the Milky Way. The scale heights of the different gas tracers, such as H I and CO, are a measure of these processes. The scale height of [C II] emission in the Galactic plane is important for understanding those ISM components not traced by CO or H I.
Aims. We determine the average distribution of [C II] perpendicular to the plane in the inner Galactic disk and compare it to the distributions of other key gas tracers, such as CO and H I.
Methods. We calculated the vertical, z, distribution of [C II] in the inner Galactic disk by adopting a model for the emission that combines the latitudinal, b, spectrally unresolved BICE survey, with the spectrally resolved Herschel Galactic plane survey of [C II] at b = 0 degrees. Our model assumed a Gaussian emissivity distribution vertical to the plane, and related the distribution in z to that of the latitude b using the spectrally resolved [C II] Herschel survey as the boundary solution for the emissivity at b = 0 degrees.
Results. We find that the distribution of [C II] perpendicular to the plane has a full-width half-maximum of 172 pc, larger than that of CO, which averages similar to 110 pc in the inner Galaxy, but smaller than that of H I, similar to 230 pc, and is offset by -28 pc.
Conclusions. We explain the difference in distributions of [C II], CO, and H I as due to [C II] tracing a mix of ISM components. Models of hydrostatic equilibrium of clouds in the disk predict different scale heights, for the same interstellar pressure. The diffuse molecular clouds with [C II] but no CO emission likely have a scale height intermediate between the low density atomic hydrogen H I clouds and the dense CO molecular clouds.
C1 [Langer, W. D.; Pineda, J. L.; Velusamy, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Langer, WD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Willlam.Langer@jpl.nasa.gov
NR 32
TC 9
Z9 9
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2014
VL 564
AR A101
DI 10.1051/0004-6361/201323281
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF4GW
UT WOS:000334671000101
ER
PT J
AU Menu, J
van Boekel, R
Henning, T
Chandler, CJ
Linz, H
Benisty, M
Lacour, S
Min, M
Waelkens, C
Andrews, SM
Calvet, N
Carpenter, JM
Corder, SA
Deller, AT
Greaves, JS
Harris, RJ
Isella, A
Kwon, W
Lazio, J
Le Bouquin, JB
Menard, F
Mundy, LG
Perez, LM
Ricci, L
Sargent, AI
Storm, S
Testi, L
Wilner, DJ
AF Menu, J.
van Boekel, R.
Henning, Th.
Chandler, C. J.
Linz, H.
Benisty, M.
Lacour, S.
Min, M.
Waelkens, C.
Andrews, S. M.
Calvet, N.
Carpenter, J. M.
Corder, S. A.
Deller, A. T.
Greaves, J. S.
Harris, R. J.
Isella, A.
Kwon, W.
Lazio, J.
Le Bouquin, J. -B.
Menard, F.
Mundy, L. G.
Perez, L. M.
Ricci, L.
Sargent, A. I.
Storm, S.
Testi, L.
Wilner, D. J.
TI On the structure of the transition disk around TW Hydrae
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE protoplanetary disks; techniques: interferometric; stars: individual: TW
Hya
ID INTERSTELLAR SILICATE MINERALOGY; HERBIG AE/BE STARS; PROTOPLANETARY
DISKS; CIRCUMSTELLAR DISKS; HD 100546; SCATTERED-LIGHT; GRAIN-GROWTH;
RADIATIVE-TRANSFER; ACCRETION DISKS; INNER HOLE
AB Context. For over a decade, the structure of the inner cavity in the transition disk of TW Hydrae has been a subject of debate. Modeling the disk with data obtained at different wavelengths has led to a variety of proposed disk structures. Rather than being inconsistent, the individual models might point to the different faces of physical processes going on in disks, such as dust growth and planet formation.
Aims. Our aim is to investigate the structure of the transition disk again and to find to what extent we can reconcile apparent model differences.
Methods. A large set of high-angular-resolution data was collected from near-infrared to centimeter wavelengths. We investigated the existing disk models and established a new self-consistent radiative-transfer model. A genetic fitting algorithm was used to automatize the parameter fitting, and uncertainties were investigated in a Bayesian framework.
Results. Simple disk models with a vertical inner rim and a radially homogeneous dust composition from small to large grains cannot reproduce the combined data set. Two modifications are applied to this simple disk model: (1) the inner rim is smoothed by exponentially decreasing the surface density in the inner similar to 3 AU, and (2) the largest grains (>100 mu m) are concentrated towards the inner disk region. Both properties can be linked to fundamental processes that determine the evolution of protoplanetary disks: the shaping by a possible companion and the different regimes of dust-grain growth, respectively.
Conclusions. The full interferometric data set from near-infrared to centimeter wavelengths requires a revision of existing models for the TW Hya disk. We present a new model that incorporates the characteristic structures of previous models but deviates in two key aspects: it does not have a sharp edge at 4 AU, and the surface density of large grains differs from that of smaller grains. This is the first successful radiative-transfer-based model for a full set of interferometric data.
C1 [Menu, J.; Waelkens, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Menu, J.; van Boekel, R.; Henning, Th.; Linz, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Chandler, C. J.; Perez, L. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Benisty, M.; Le Bouquin, J. -B.; Menard, F.] CNRS UJF Grenoble 1, UMR 5274, Inst Planetol & Astrophys Grenoble, F-38041 Grenoble, France.
[Lacour, S.] Univ Paris Diderot, CNRS, UPMC, LESIA,Observ Paris, F-92195 Meudon, France.
[Min, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Andrews, S. M.; Harris, R. J.; Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Calvet, N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Carpenter, J. M.; Isella, A.; Ricci, L.; Sargent, A. I.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Corder, S. A.] Joint ALMA Observ, Santiago 7630000, Chile.
[Deller, A. T.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Greaves, J. S.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Kwon, W.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands.
[Lazio, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
[Menard, F.] Univ Chile, CNRS INSU France UMI 3386, UMI FCA, Santiago, Chile.
[Menard, F.] Univ Chile, Dept Astron, Santiago, Chile.
[Mundy, L. G.; Storm, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Testi, L.] European So Observ, D-85748 Garching, Germany.
[Testi, L.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
RP Menu, J (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Louvain, Belgium.
EM jonathan.menu@ster.kuleuven.be
OI Deller, Adam/0000-0001-9434-3837
FU FWO travel grant [V448412N]; Millennium Science Initiative (Chilean
Ministry of Economy) [Nucleus P10-022F]; EU FP7 [284405]; Smithsonian
Institution; Academia Sinica
FX J. Menu wishes to thank B. Acke for useful discussions, K. Johnston for
support with the CASA software, and P. Degroote for providing SED
analysis/fitting software. We are grateful to I. Pascucci and to the
anonymous referee for comments that helped improving the manuscript. J.
Menu acknowledges an FWO travel grant for a long research stay abroad
(V448412N). F. Menard acknowledges support from the Millennium Science
Initiative (Chilean Ministry of Economy), through grant "Nucleus
P10-022F". F. Menard also acknowledges funding from the EU FP7-2011
under Grant Agreement No 284405. The Submillimeter Array is a joint
project between the Smithsonian Astrophysical Observatory and the
Academia Sinica Institute of Astronomy and Astrophysics and is funded by
the Smithsonian Institution and the Academia Sinica. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
NR 126
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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 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2014
VL 564
AR A93
DI 10.1051/0004-6361/201322961
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF4GW
UT WOS:000334671000093
ER
PT J
AU Rauch, T
Werner, K
Quinet, P
Kruk, JW
AF Rauch, T.
Werner, K.
Quinet, P.
Kruk, J. W.
TI Stellar laboratories II. New Zn IV and Zn V oscillator strengths and
their validation in the hot white dwarfs G191-B2B and RE 0503-289
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE atomic data; line: identification; stars: abundances; stars: individual:
G191-B2B; virtual observatory tools; stars: individual: RE 0503-289
ID SPECTRAL-ANALYSIS; PHOTOSPHERES
AB Context. For the spectral analysis of high-resolution and high-signal-to-noise (S/N) spectra of hot stars, state-of-the-art non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that is used for their calculation. In a recent analysis of the ultraviolet (UV) spectrum of the DA-type white dwarf G191-B2B, 21 Zn IV lines were newly identified. Because of the lack of Zn IV data, transition probabilities of the isoelectronic Ge VI were adapted for a first, coarse determination of the photospheric Zn abundance.
Aims. Reliable Zn IV and Zn V oscillator strengths are used to improve the Zn abundance determination and to identify more Zn lines in the spectra of G191-B2B and the DO-type white dwarf RE 0503-289.
Methods. We performed new calculations of Zn IV and Zn V oscillator strengths to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models for the analysis of the in Zn IV - V spectrum exhibited in high-resolution and high-S/N UV observations of G191-B2B and RE 0503-289.
Results. In the UV spectrum of G191-B2B, we identify 31 Zn IV and 16 Zn V lines. Most of these are identified for the first time in any star. We can reproduce well almost all of them at log Zn = -5.52 +/- 0.2 (mass fraction, about 1.7 times solar). In particular, the in Zn IV / Zn V ionization equilibrium, which is a very sensitive T-eff indicator, is well reproduced with the previously determined T-eff = 60 000 +/- 2000 K and log g = 7.60 +/- 0.05. In the spectrum of RE 0503-289, we identified 128 Zn V lines for the first time and determined log Zn = -3.57 +/- 0.2 (155 times solar).
Conclusions. Reliable measurements and calculations of atomic data are a pre-requisite for stellar-atmosphere modeling. Observed Zn IV and Zn V line profiles in two white dwarf (G191-B2B and RE 0503-289) ultraviolet spectra were well reproduced with our newly calculated oscillator strengths. This allowed us to determine the photospheric Zn abundance of these two stars precisely.
C1 [Rauch, T.; Werner, K.] Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany.
[Quinet, P.] Univ Mons UMONS, B-7000 Mons, Belgium.
[Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium.
[Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rauch, T (reprint author), Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, Sand 1, D-72076 Tubingen, Germany.
EM rauch@astro.uni-tuebingen.de
FU German Aerospace Center (DLR) [05 OR 0806]; Belgian FRS-FNRS; NASA
[NAS5-26555]; NASA Office of Space Science [NNX09AF08G]
FX T.R. is supported by the German Aerospace Center (DLR, grant 05 OR
0806). Financial support from the Belgian FRS-FNRS is also acknowledged.
PQ is research director of this organization. This research has made use
of the SIMBAD database, operated at CDS, Strasbourg, France. 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 10
TC 11
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U1 1
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2014
VL 564
AR A41
DI 10.1051/0004-6361/201423491
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF4GW
UT WOS:000334671000041
ER
PT J
AU Schonherr, G
Schwarm, FW
Falkner, S
Dauser, T
Ferrigno, C
Kuhnel, M
Klochkov, D
Kretschmar, P
Becker, PA
Wolff, MT
Pottschmidt, K
Falanga, M
Kreykenbohm, I
Furst, F
Staubert, R
Wilms, J
AF Schoenherr, G.
Schwarm, F. -W.
Falkner, S.
Dauser, T.
Ferrigno, C.
Kuehnel, M.
Klochkov, D.
Kretschmar, P.
Becker, P. A.
Wolff, M. T.
Pottschmidt, K.
Falanga, M.
Kreykenbohm, I.
Fuerst, F.
Staubert, R.
Wilms, J.
TI Formation of phase lags at the cyclotron energies in the pulse profiles
of magnetized, accreting neutron stars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: binaries; stars: neutron; methods: numerical
ID X-RAY PULSARS; BEAM PATTERN; CENTAURUS X-3; 4U 0115+63; GEOMETRY;
SCATTERING; LINE; RADIATION; FEATURES; SPECTRA
AB Context. Accretion-powered X-ray pulsars show highly energy-dependent and complex pulse-profile morphologies. Significant deviations from the average pulse profile can appear, in particular close to the cyclotron line energies. These deviations can be described as energy-dependent phase lags, that is, as energy-dependent shifts of main features in the pulse profile.
Aims. Using a numerical study we explore the effect of cyclotron resonant scattering on observable, energy-resolved pulse profiles.
Methods. We generated the observable emission as a function of spin phase, using Monte Carlo simulations for cyclotron resonant scattering and a numerical ray-tracing routine accounting for general relativistic light-bending effects on the intrinsic emission from the accretion columns.
Results. We find strong changes in the pulse profile coincident with the cyclotron line energies. Features in the pulse profile vary strongly with respect to the average pulse profile with the observing geometry and shift and smear out in energy additionally when assuming a non-static plasma.
Conclusions. We demonstrate how phase lags at the cyclotron energies arise as a consequence of the effects of angular redistribution of X-rays by cyclotron resonance scattering in a strong magnetic field combined with relativistic effects. We also show that phase lags are strongly dependent on the accretion geometry. These intrinsic effects will in principle allow us to constrain a system's accretion geometry.
C1 [Schoenherr, G.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
[Schoenherr, G.; Schwarm, F. -W.; Falkner, S.; Dauser, T.; Kuehnel, M.; Kreykenbohm, I.; Wilms, J.] Dr Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany.
[Ferrigno, C.] Univ Geneva, INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Klochkov, D.; Staubert, R.] Univ Tubingen, Abt Astron, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Kretschmar, P.] European Space Astron Ctr ESA ESAC, Sci Operat Dept, Madrid 28691, Spain.
[Becker, P. A.] George Mason Univ, Fairfax, VA 22030 USA.
[Wolff, M. T.] Naval Res Lab, Div Space Sci, High Energy Space Environm Branch, Washington, DC 20375 USA.
[Pottschmidt, K.] Univ Maryland Baltimore Cty, CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Falanga, M.] Int Space Sci Inst, CH-3012 Bern, Switzerland.
[Fuerst, F.] CALTECH, Pasadena, CA 91125 USA.
RP Schonherr, G (reprint author), Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany.
EM g.schoenherr@aip.de
RI Wilms, Joern/C-8116-2013;
OI Wilms, Joern/0000-0003-2065-5410; Falkner,
Sebastian/0000-0001-5209-991X; Kretschmar, Peter/0000-0001-9840-2048
FU Bundesministerium fur Wirtschaft und Technologie through Deutsches
Zentrum fur Luft- und Raumfahrt [50 OR 1113]; US Office of Naval
Research; NASA ADAP Program [NNH13AV18I]
FX We thank the International Space Science Institute ISSI in Bern (CH) for
granting two International Team meetings on "The physics of the
accretion column of X-ray pulsars", which have much inspired this
collaborative work. We also thank the Bundesministerium fur Wirtschaft
und Technologie for funding through Deutsches Zentrum fur Luft- und
Raumfahrt grant 50 OR 1113. M.T.W. is supported by the US Office of
Naval Research and the NASA ADAP Program under grant NNH13AV18I. We
thank the anonymous referee for very useful comments.
NR 27
TC 5
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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 APR
PY 2014
VL 564
AR L8
DI 10.1051/0004-6361/201322448
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AF4GW
UT WOS:000334671000147
ER
PT J
AU Wu, SC
Remington, RW
Folk, CL
AF Wu, Shu-Chieh
Remington, Roger W.
Folk, Charles L.
TI Onsets do not override top-down goals, but they are responded to more
quickly
SO ATTENTION PERCEPTION & PSYCHOPHYSICS
LA English
DT Article
DE Attentional capture; Visual search; Selective attention
ID ABRUPT ONSETS; PRIORITIZING SELECTION; CONTROL SETTINGS;
STIMULUS-DRIVEN; VISUAL MARKING; CAPTURE; ATTENTION; ADDITIVITY; SEARCH;
COVERT
AB Do onsets automatically capture attention? Spatial-cuing experiments often reveal no capture by onset cues in searches for color targets. However, recent experiments have shown faster responses to an uncued color target presented as an abrupt onset than as a change to an existing item, which has been argued to reflect capture by the onset. In the present experiment, we tested whether this onset advantage reflects the capture of attention or processing independent of shifts of attention. In a modified spatial-cuing paradigm, noninformative color precues were paired with color targets presented as abrupt onsets or as no-onset characters. Critically, the number of other onset items in the target display was manipulated, which has previously been shown to disrupt attention allocation to any particular item. It was reasoned that if the onset advantage for uncued color targets reflects attentional capture, then the appearance of additional onsets should eliminate this advantage. The results showed that even with multiple onsets on the target display, the onset advantage remained additive with cue validity. The additive effects are inconsistent with automatic capture by onsets, suggesting instead that the onset advantage arises from an independent source.
C1 [Wu, Shu-Chieh] San Jose State Univ, Moffett Field, CA 94035 USA.
[Wu, Shu-Chieh] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Remington, Roger W.] Univ Queensland, St Lucia, Qld, Australia.
[Folk, Charles L.] Villanova Univ, Villanova, PA 19085 USA.
RP Wu, SC (reprint author), San Jose State Univ, Mail Stop 262-4, Moffett Field, CA 94035 USA.
EM shu-chieh.wu@nasa.gov
FU Australian Research Council Discovery Grant [DP120103721]
FX R.W.R. and C.L.F. were supported by Australian Research Council
Discovery Grant No. DP120103721. Portions of this article were presented
at the 52nd Annual Meeting of the Psychonomic Society, Seattle,
Washington, November 2011. We thank Alexandra Shelley for her assistance
in recruiting and testing participants, and two anonymous reviewers for
comments on the manuscript.
NR 17
TC 5
Z9 6
U1 0
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1943-3921
EI 1943-393X
J9 ATTEN PERCEPT PSYCHO
JI Atten. Percept. Psychophys.
PD APR
PY 2014
VL 76
IS 3
BP 649
EP 654
DI 10.3758/s13414-014-0637-z
PG 6
WC Psychology; Psychology, Experimental
SC Psychology
GA AF2CX
UT WOS:000334521300001
PM 24596080
ER
PT J
AU Perrot, D
Molotch, NP
Musselman, KN
Pugh, ET
AF Perrot, Danielle
Molotch, Noah P.
Musselman, Keith N.
Pugh, Evan T.
TI Modelling the effects of the mountain pine beetle on snowmelt in a
subalpine forest
SO ECOHYDROLOGY
LA English
DT Article
DE snow-vegetation interactions; mountain pine beetle; snowmelt modeling;
tree death
ID BOREAL FOREST; ENERGY-BALANCE; NIWOT RIDGE; ACCUMULATION; RADIATION;
ABLATION; CANOPY; SOIL; STREAMFLOW; EPIDEMIC
AB The recent mountain pine beetle epidemic in the Colorado River Basin has resulted in widespread tree mortality in pine stands across the Colorado Plateau. Because of complex micro-scale (i.e. tree well scale) interactions between vegetation and snow processes, one of the most significant issues resulting from this epidemic is the potential hydrologic impacts of the effects of changing forest structure. Using SNTHERM, we conducted a comparative modelling scenario analysis of the snowpack along a transect between two trees over the course of the snow ablation season (28 February-30 June) under four forest stand conditions to assess changes in snowpack characteristics because of loss of canopy biomass. We found that the red phase scenario (intermediate phase of tree death) exhibited a 4-day earlier snow disappearance date than the living stand scenario and grey phase scenario (advanced phase of tree death), although the timing of isothermal conditions at 0 degrees C was identical. The modelled clearcut scenario snowpack became isothermal at 0 degrees C 10days earlier than the living, red phase, or grey phase scenarios. The clearcut modelling scenario also exhibited the greatest homogenization of snow properties, and the spatio-temporal distribution of snow disappearance at the tree well scale was 70% as variable as the living, red phase and grey phase modelling scenarios. These results provide insight to the processes responsible for changing hydrologic dynamics in snow-dominated forest ecosystems with the onset of vegetation stress and death and may help inform future forest management strategies. Copyright (c) 2012 John Wiley & Sons, Ltd.
C1 [Perrot, Danielle; 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.
[Musselman, Keith N.] Univ Calif Los Angeles, Dept Civil & Environm Engn, Los Angeles, CA USA.
[Pugh, Evan T.] Univ Colorado, Dept Geol, Boulder, CO 80309 USA.
RP Perrot, D (reprint author), Univ Colorado, Dept Geog, Inst Arctic & Alpine Res Campus,Box 450, Boulder, CO 80309 USA.
EM danielle.perrot@colorado.edu
RI Molotch, Noah/C-8576-2009
FU National Science Foundation Hydrological Sciences grants [EAR1032295,
EAR1032308, EAR 1141764]
FX This project was funded by the National Science Foundation Hydrological
Sciences grants EAR1032295, EAR1032308, and EAR 1141764. Many thanks to
Sean Burns, Mark Williams and Christopher Knight.
NR 61
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U1 1
U2 18
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1936-0584
EI 1936-0592
J9 ECOHYDROLOGY
JI Ecohydrology
PD APR
PY 2014
VL 7
IS 2
BP 226
EP 241
DI 10.1002/eco.1329
PG 16
WC Ecology; Environmental Sciences; Water Resources
SC Environmental Sciences & Ecology; Water Resources
GA AF4HC
UT WOS:000334671600005
ER
PT J
AU Jee, S
Shariff, K
AF Jee, SolKeun
Shariff, Karim
TI Detached-eddy simulation based on the v(2) - f model
SO INTERNATIONAL JOURNAL OF HEAT AND FLUID FLOW
LA English
DT Article
DE Detached-eddy simulation; v(2) - f model; Hybrid RANS/LES
ID CIRCULAR-CYLINDER; TURBULENCE MODEL; ISOTROPIC TURBULENCE; FLOW;
CHANNELS; CLOSURE; WAKE
AB Detached-eddy simulation (DES) based on the v(2) - f Reynolds-averaged Navier-Stokes (RANS) model is developed and tested. The v(2) - f model incorporates anisotropy of near-wall turbulence, which is absent in other RANS models commonly used for DES. The v(2) - f RANS model is modified in order that in the DES formulation it reduces to a transport equation for the subgrid-scale kinetic energy in isotropic turbulence. First, three coefficients in the elliptic relaxation equation are modified and the modification is tested for RANS of channel flow. Next, the proposed v(2) - f DES model is formulated. The constant, Cam, required in the DES formulation is calibrated by simulating both decaying and statistically-steady isotropic turbulence. The formulation is tested for flow around a circular cylinder at a Reynolds number of 3900, in which case turbulence develops after separation. Simulations indicate that this model represents the turbulent wake nearly as accurately as the dynamic Smagorinsky model. For comparison, Spalart-Allmaras (SA) based DES is also included in the cylinder flow simulations. Finally, the proposed model is tested for a separated turbulent boundary layer on an airfoil. The delayed-DES (DDES) approach is found to be necessary. The v(2) - f DDES calculation gives good predictions for the aerodynamic forces and the pressure distribution measured in experiments. The proposed model is also compared with SA-DDES for the airfoil. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Jee, SolKeun; Shariff, Karim] NASA, Ames Res Ctr, Moffett Field, CA 94043 USA.
RP Jee, S (reprint author), United Technol Res Ctr, 411 Silver Lane,MS 129-89, E Hartford, CT 06108 USA.
EM jees@utrc.utc.com; karim.shariff@nasa.gov
OI Shariff, Karim/0000-0002-7256-2497
FU SolKeun Jee to the NASA Postdoctoral Program at the Ames Research Center
FX The authors thank Dr. Michael Rogers and Dr. Scott Murman of NASA Ames
Research Center for helpful discussions and their suggestions on a draft
version of the manuscript. This research was supported by appointment of
SolKeun Jee to the NASA Postdoctoral Program at the Ames Research
Center, administered by Oak Ridge Associated Universities through a
contract with NASA.
NR 48
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U1 0
U2 18
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0142-727X
EI 1879-2278
J9 INT J HEAT FLUID FL
JI Int. J. Heat Fluid Flow
PD APR
PY 2014
VL 46
BP 84
EP 101
DI 10.1016/j.ijheatfluidflow.2013.12.006
PG 18
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA AG0KA
UT WOS:000335103200007
ER
PT J
AU Das, S
Louis, T
Nolta, MR
Addison, GE
Battistelli, ES
Bond, JR
Calabrese, E
Crichton, D
Devlin, MJ
Dicker, S
Dunkley, J
Dunner, R
Fowler, JW
Gralla, M
Hajian, A
Halpern, M
Hasselfield, M
Hilton, M
Hincks, AD
Hlozek, R
Huffenberger, KM
Hughes, JP
Irwin, KD
Kosowsky, A
Lupton, RH
Marriage, TA
Marsden, D
Menanteau, F
Moodley, K
Niemack, MD
Page, LA
Partridge, B
Reese, ED
Schmitt, BL
Sehgal, N
Sherwin, BD
Sievers, JL
Spergel, DN
Staggs, ST
Swetz, DS
Switzer, ER
Thornton, R
Trac, H
Wollack, E
AF Das, Sudeep
Louis, Thibaut
Nolta, Michael R.
Addison, Graeme E.
Battistelli, Elia S.
Bond, J. Richard
Calabrese, Erminia
Crichton, Devin
Devlin, Mark J.
Dicker, Simon
Dunkley, Joanna
Duenner, Rolando
Fowler, Joseph W.
Gralla, Megan
Hajian, Amir
Halpern, Mark
Hasselfield, Matthew
Hilton, Matt
Hincks, Adam D.
Hlozek, Renee
Huffenberger, Kevin M.
Hughes, John P.
Irwin, Kent D.
Kosowsky, Arthur
Lupton, Robert H.
Marriage, Tobias A.
Marsden, Danica
Menanteau, Felipe
Moodley, Kavilan
Niemack, Michael D.
Page, Lyman A.
Partridge, Bruce
Reese, Erik D.
Schmitt, Benjamin L.
Sehgal, Neelima
Sherwin, Blake D.
Sievers, Jonathan L.
Spergel, David N.
Staggs, Suzanne T.
Swetz, Daniel S.
Switzer, Eric R.
Thornton, Robert
Trac, Hy
Wollack, Ed
TI The Atacama Cosmology Telescope: temperature and gravitational lensing
power spectrum measurements from three seasons of data
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE CMBR experiments; gravitational lensing; Sunyaev-Zeldovich effect; CMBR
theory
ID SOUTH-POLE TELESCOPE; MICROWAVE BACKGROUND ANISOTROPIES; DAMPING TAIL;
148 GHZ; MAPS; CONSTRAINTS; PARAMETERS; SCALE; FIELD; QUAD
AB We present the temperature power spectra. of the cosmic microwave background (CMD) derived from the three seasons of data from the Atacama Cosmology Telescope (ACT) at 148 Ealiz and 218 GHz as well as the (Toss-frequency spectrum between the two channels. We detect and correct. for contamination due to the Galactic cirrus in our equatorial maps. We present the results of a number of tests for possible systematic error and conclude that any effects are not significant compared to the statistical errors we quote. Where they overlap we cross-correlate the ACT and the South Pole Telescope (APT) maps and show they are consistent. The measurements of higher-order peaks in the CMB power spectrum provide an additional test of the ACDM cosmological model, and help constrain extensions beyond the standard model. The small angular scale power sped rum also provides constraining power on the Sunyaev-Zel'clovich effects and extragalactic foregrounds. We also present a measurement of the CMB gravitational lensing convergence power spectrum at 4.6 sigma detection significance.
C1 [Das, Sudeep] Argonne Natl Lab, Lemont, IL 60439 USA.
[Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA.
[Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Louis, Thibaut; Addison, Graeme E.; Calabrese, Erminia; Dunkley, Joanna] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England.
[Nolta, Michael R.; Bond, J. Richard; Hajian, Amir; Hincks, Adam D.; Sievers, Jonathan L.; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Addison, Graeme E.; Battistelli, Elia S.; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Crichton, Devin; Gralla, Megan; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Devlin, Mark J.; Dicker, Simon; Marsden, Danica; Reese, Erik D.; Schmitt, Benjamin L.; Thornton, Robert] Univ Penn, Dept Astron & Astrophys, Philadelphia, PA 19104 USA.
[Duenner, Rolando] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Fowler, Joseph W.; Niemack, Michael D.; Swetz, Daniel S.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA.
[Fowler, Joseph W.; Niemack, Michael D.; Page, Lyman A.; Sherwin, Blake D.; Sievers, Jonathan L.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Hasselfield, Matthew; Hlozek, Renee; Marriage, Tobias A.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England.
[Hilton, Matt; Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Marsden, Danica] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA.
[Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Sehgal, Neelima] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Thornton, Robert] West Chester Univ Pennsylvania, Dept Phys, W Chester, PA 19383 USA.
[Trac, Hy] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Das, S (reprint author), Argonne Natl Lab, 9700 S Cass Ave, Lemont, IL 60439 USA.
EM sudeepphys@gmail.com
RI Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012;
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
Huffenberger, Kevin/0000-0001-7109-0099; Menanteau,
Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074
FU U.S. National Science Foundation [AST-0408698, AST-0965625]; ACT project
[PHY-0855887, PHY-1214379]; Princeton University; University of
Pennsylvania; Canada Foundation for Innovation (CFI) award; Comision
Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT);
CFI; Compute Canada; Government of Ontario; Ontario Research Fund -
Research Excellence; University of Toronto; David Schramm Fellowship at
Argonne National Laboratory; Berkeley Center for Cosmological Physics
fellowship; FONDECYT grant; BASAL grant
FX This work was supported by the U.S. National Science Foundation through
awards AST-0408698 and AST-0965625 for the ACT project, as well as
awards PHY-0855887 and PHY-1214379. Funding was also provided by
Princeton University, the University of Pennsylvania, and a Canada
Foundation for Innovation (CFI) award to ITBC. ACT operates in the
Parque Astronomico Atacama in northern Chile under the auspices of the
Comision Nacional de Investigacion Cientifica y Tecnologica de Chile
(CONICYT). Computations were performed on the GPC supercomputer at the
SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of
Compute Canada, the Government of Ontario, the Ontario Research Fund -
Research Excellence; and the University of Toronto. SD acknowledges
support from the David Schramm Fellowship at Argonne National Laboratory
and the Berkeley Center for Cosmological Physics fellowship. RD
acknowledges support from FONDECYT and BASAL grants.
NR 47
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U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD APR
PY 2014
IS 4
AR 014
DI 10.1088/1475-7516/2014/04/014
PG 36
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AF1TK
UT WOS:000334496500014
ER
PT J
AU Sears, DWG
AF Sears, Derek W. G.
TI Oral histories in meteoritics and planetary science - XXII: John T.
Wasson
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID IRON METEORITES; CHONDRITES; ORIGIN; CHONDRULES; GERMANIUM; GALLIUM;
MAGMA; MELT
AB Abstract
In this interview, John Wasson (Fig. ) describes his childhood and undergraduate years in Arkansas and his desire to pursue nuclear chemistry as a graduate student at MIT. Upon graduation, John spent time in Munich (Technische Hochschule), the Air Force Labs in Cambridge, MA, and a sabbatical at the University of Bern where he developed his interests in meteorites. Upon obtaining his faculty position at UCLA, John established a neutron activation laboratory and began a long series of projects on the bulk compositions of iron meteorites and chondrites. He developed the chemical classification scheme for iron meteorites, gathered a huge set of iron meteorite compositional data with resultant insights into their formation, and documented the refractory and moderately volatile element trends that characterize the chondrites and chondrules. He also spent several years studying field relations and compositions of layered tektites from Southeast Asia, proposing an origin by radiant heating from a mega-Tunguska explosion. Recently, John has explored oxygen isotope patterns in meteorites and their constituents believing the oxygen isotope results to be some of the most important discoveries in cosmochemistry. John also describes the role of postdoctoral colleagues and their important work, his efforts in the reorganization and modernization of the Meteoritical Society, his contributions in reshaping the journal Meteoritics, and how, with UCLA colleagues, he organized two meetings of the society. John Wasson earned the Leonard Medal of the Meteoritical Society in 1992 and the J. Lawrence Smith Medal of the National Academy in 2003.
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, MS245-3, Mountain View, CA 94035 USA.
EM derek.sears@nasa.gov
FU NASA
FX This interview was recorded on February 6th, 2013, and edited by the
author and JW. I am grateful to NASA for financial support and to John
Friedrich and Hazel Sears for reviews, and Hazel also for proofing.
NR 21
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U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD APR
PY 2014
VL 49
IS 4
BP 706
EP 721
DI 10.1111/maps.12266
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AF4KG
UT WOS:000334680200013
ER
PT J
AU Nicolau, E
Fonseca, JJ
Rodriguez-Martinez, JA
Richardson, TMJ
Flynn, M
Griebenow, K
Cabrera, CR
AF Nicolau, Eduardo
Fonseca, Jose J.
Rodriguez-Martinez, Jose A.
Richardson, Tra-My Justine
Flynn, Michael
Griebenow, Kai
Cabrera, Carlos R.
TI Evaluation of a Urea Bioelectrochemical System for Wastewater Treatment
Processes
SO ACS SUSTAINABLE CHEMISTRY & ENGINEERING
LA English
DT Article
DE Resource recovery; Water reclamation; Urea degradation; Electrochemical
cell; Bioreactor
ID AMMONIA ELECTROLYSIS; HYDROGEN-PRODUCTION; RECLAMATION; DEGRADATION;
CREATININE; OXIDATION; PLATINUM; OSMOSIS; PHENOL
AB Due to the high cost of delivering supplies to space, the recovery of potable water from spacecraft wastewater is critical for life support of crewmembers in short- and long-term missions. It is estimated that in future long-term space missions, human wastes such as urine will contribute more than 50% of the total waste. Thus, we will demonstrate how unused components, such as urea, can be recovered and reused in wastewater recycling processes. In this system, a urea bioreactor (GAC-urease) converts urea to ammonia. Then, an electrochemical cell converts the ammonia to power. The combined system is referred to as the Urea Bioreactor Electrochemical (UBE) unit. The results of this research showed the feasibility of interfacing wastewater-recycling processes with bioelectrochemical systems to achieve water recycling while reusing useful resources. The UBE systems removed > 80% of organic carbons and converted approximately 86% of the urea to ammonia. Therefore, the concept herein proposed has the potential to be used in water recycling applications with emphasis in contaminant recovery from wastewater for useful resources and energy.
C1 [Nicolau, Eduardo; Fonseca, Jose J.; Rodriguez-Martinez, Jose A.; Griebenow, Kai; Cabrera, Carlos R.] Univ Puerto Rico, Dept Chem, San Juan, PR 00931 USA.
[Nicolau, Eduardo; Fonseca, Jose J.; Rodriguez-Martinez, Jose A.; Griebenow, Kai; Cabrera, Carlos R.] Univ Puerto Rico, NASA Ctr Adv Nanoscale Mat, San Juan, PR 00931 USA.
[Nicolau, Eduardo; Cabrera, Carlos R.] Univ Puerto Rico, Sect El Cinco, San Juan, PR 00926 USA.
[Richardson, Tra-My Justine; Flynn, Michael] NASA, Bioengn Branch, Ames Res Ctr, Mountain View, CA 94036 USA.
RP Nicolau, E (reprint author), Univ Puerto Rico, Dept Chem, Rio Piedras Campus,POB 23346, San Juan, PR 00931 USA.
EM eduardo.nicolau@upr.edu; carlos.cabrera2@upr.edu
RI Rodriguez-Martinez, Jose/F-3554-2010;
OI Rodriguez-Martinez, Jose/0000-0002-1191-2887; Cabrera,
Carlos/0000-0002-3342-8666
FU NASA Center for Advanced Nanoscale Materials [NNX08BA48A, NNX13AD20A];
NASA Graduate Student Researchers Program [NNX08AV42H]
FX This work was financially supported in part by the NASA Center for
Advanced Nanoscale Materials under Grant NNX08BA48A, NNX13AD20A, and the
NASA Graduate Student Researchers Program under Grant NNX08AV42H. The
authors are also grateful to David Beeler for comments and editing and
Kevin Howard.
NR 26
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U2 51
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 2168-0485
J9 ACS SUSTAIN CHEM ENG
JI ACS Sustain. Chem. Eng.
PD APR
PY 2014
VL 2
IS 4
BP 749
EP 754
DI 10.1021/sc400342x
PG 6
WC Chemistry, Multidisciplinary; GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY;
Engineering, Chemical
SC Chemistry; Science & Technology - Other Topics; Engineering
GA AE6IA
UT WOS:000334092600026
ER
PT J
AU Armstrong, JC
Barnes, R
Domagal-Goldman, S
Breiner, J
Quinn, TR
Meadows, VS
AF Armstrong, J. C.
Barnes, R.
Domagal-Goldman, S.
Breiner, J.
Quinn, T. R.
Meadows, V. S.
TI Effects of Extreme Obliquity Variations on the Habitability of
Exoplanets
SO ASTROBIOLOGY
LA English
DT Article
ID PLANET-PLANET SCATTERING; MAIN-SEQUENCE STARS; CLIMATE MODEL;
ECCENTRICITY; ZONE; STABILIZATION; CATALOG; SYSTEMS; EARTH
AB We explore the impact of obliquity variations on planetary habitability in hypothetical systems with high mutual inclination. We show that large-amplitude, high-frequency obliquity oscillations on Earth-like exoplanets can suppress the ice-albedo feedback, increasing the outer edge of the habitable zone. We restricted our exploration to hypothetical systems consisting of a solar-mass star, an Earth-mass planet at 1 AU, and 1 or 2 larger planets. We verified that these systems are stable for 10(8) years with N-body simulations and calculated the obliquity variations induced by the orbital evolution of the Earth-mass planet and a torque from the host star. We ran a simplified energy balance model on the terrestrial planet to assess surface temperature and ice coverage on the planet's surface, and we calculated differences in the outer edge of the habitable zone for planets with rapid obliquity variations. For each hypothetical system, we calculated the outer edge of habitability for two conditions: (1) the full evolution of the planetary spin and orbit and (2) the eccentricity and obliquity fixed at their average values. We recovered previous results that higher values of fixed obliquity and eccentricity expand the habitable zone, but we also found that obliquity oscillations further expand habitable orbits in all cases. Terrestrial planets near the outer edge of the habitable zone may be more likely to support life in systems that induce rapid obliquity oscillations as opposed to fixed-spin planets. Such planets may be the easiest to directly characterize with space-borne telescopes. Key Words: Exoplanets-Habitable zone-Energy balance models. Astrobiology 14, 277-291.
C1 [Armstrong, J. C.] Weber State Univ, Dept Phys, Ogden, UT 84408 USA.
[Barnes, R.; Breiner, J.; Quinn, T. R.; Meadows, V. S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Domagal-Goldman, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Armstrong, JC (reprint author), Weber State Univ, Dept Phys, Ogden, UT 84408 USA.
EM jcarmstrong@weber.edu
FU NASA Astrobiology Institute's Virtual Planetary Lab lead team; NAI
Director's Discretionary Fund
FX This work was supported by the NASA Astrobiology Institute's Virtual
Planetary Lab lead team and an award from the NAI Director's
Discretionary Fund.
NR 44
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U1 2
U2 12
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 APR 1
PY 2014
VL 14
IS 4
BP 277
EP 291
DI 10.1089/ast.2013.1129
PG 15
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA AF0UX
UT WOS:000334430700002
PM 24611714
ER
PT J
AU Marlow, JJ
LaRowe, DE
Ehlmann, BL
Amend, JP
Orphan, VJ
AF Marlow, Jeffrey J.
LaRowe, Douglas E.
Ehlmann, Bethany L.
Amend, Jan P.
Orphan, Victoria J.
TI The Potential for Biologically Catalyzed Anaerobic Methane Oxidation on
Ancient Mars
SO ASTROBIOLOGY
LA English
DT Article
ID PARTIAL MOLAL PROPERTIES; YELLOWSTONE-NATIONAL-PARK; SEA HYDROTHERMAL
SYSTEMS; MEXICO COLD SEEPS; HIGH-PRESSURES; SULFATE REDUCTION;
THERMODYNAMIC PROPERTIES; GEOCHEMICAL CONSTRAINTS; TRANSPORT-PROPERTIES;
MERIDIANI-PLANUM
AB This study examines the potential for the biologically mediated anaerobic oxidation of methane (AOM) coupled to sulfate reduction on ancient Mars. Seven distinct fluids representative of putative martian groundwater were used to calculate Gibbs energy values in the presence of dissolved methane under a range of atmospheric CO2 partial pressures. In all scenarios, AOM is exergonic, ranging from -31 to -135 kJ/mol CH4. A reaction transport model was constructed to examine how environmentally relevant parameters such as advection velocity, reactant concentrations, and biomass production rate affect the spatial and temporal dependences of AOM reaction rates. Two geologically supported models for ancient martian AOM are presented: a sulfate-rich groundwater with methane produced from serpentinization by-products, and acid-sulfate fluids with methane from basalt alteration. The simulations presented in this study indicate that AOM could have been a feasible metabolism on ancient Mars, and fossil or isotopic evidence of this metabolic pathway may persist beneath the surface and in surface exposures of eroded ancient terrains. Key Words: Mars-Methanotrophy-Methane. Astrobiology 14, 292-307.
C1 [Marlow, Jeffrey J.; Ehlmann, Bethany L.; Orphan, Victoria J.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[LaRowe, Douglas E.; Amend, Jan P.] Univ So Calif, Dept Earth Sci, Los Angeles, CA USA.
[Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Amend, Jan P.] Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA.
RP Marlow, JJ (reprint author), CALTECH, Div Geol & Planetary Sci, 1200 E Calif Ave,MC 100-23, Pasadena, CA 91125 USA.
EM jjmarlow@caltech.edu
RI Orphan, Victoria/K-1002-2014
OI Orphan, Victoria/0000-0002-5374-6178
FU NETL-National Academy of Sciences Methane Hydrate Research Fellowship;
Life Underground NASA Astrobiology Institute (NAI) based at USC
FX J.J.M. would like to thank Dawn Cardace, Andrew Dale, and Megan Newcombe
for helpful discussion and consultation and the NETL-National Academy of
Sciences Methane Hydrate Research Fellowship for financial support.
D.E.L. and J.P.A. would like to acknowledge financial support from the
Life Underground NASA Astrobiology Institute (NAI) based at USC. V.J.O.
acknowledges the Penn State Astrobiology Research Center NAI.
NR 149
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U1 1
U2 31
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 APR 1
PY 2014
VL 14
IS 4
BP 292
EP 307
DI 10.1089/ast.2013.1078
PG 16
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA AF0UX
UT WOS:000334430700003
PM 24684241
ER
PT J
AU Russell, MJ
Barge, LM
Bhartia, R
Bocanegra, D
Bracher, PJ
Branscomb, E
Kidd, R
McGlynn, S
Meier, DH
Nitschke, W
Shibuya, T
Vance, S
White, L
Kanik, I
AF Russell, Michael J.
Barge, Laura M.
Bhartia, Rohit
Bocanegra, Dylan
Bracher, Paul J.
Branscomb, Elbert
Kidd, Richard
McGlynn, Shawn
Meier, David H.
Nitschke, Wolfgang
Shibuya, Takazo
Vance, Steve
White, Lauren
Kanik, Isik
TI The Drive to Life on Wet and Icy Worlds
SO ASTROBIOLOGY
LA English
DT Article
ID CITY HYDROTHERMAL FIELD; RESPIRATORY COMPLEX I; INSOLUBLE
ORGANIC-MATTER; EARTHS EARLY ATMOSPHERE; MID-ATLANTIC RIDGE;
NUVVUAGITTUQ SUPRACRUSTAL BELT; MINERAL INDUCED FORMATION; IRON-SULFUR
CLUSTERS; SULFATE GREEN RUST; PREBIOTIC SYNTHESIS
AB This paper presents a reformulation of the submarine alkaline hydrothermal theory for the emergence of life in response to recent experimental findings. The theory views life, like other self-organizing systems in the Universe, as an inevitable outcome of particular disequilibria. In this case, the disequilibria were two: (1) in redox potential, between hydrogen plus methane with the circuit-completing electron acceptors such as nitrite, nitrate, ferric iron, and carbon dioxide, and (2) in pH gradient between an acidulous external ocean and an alkaline hydrothermal fluid. Both CO2 and CH4 were equally the ultimate sources of organic carbon, and the metal sulfides and oxyhydroxides acted as protoenzymatic catalysts. The realization, now 50 years old, that membrane-spanning gradients, rather than organic intermediates, play a vital role in life's operations calls into question the idea of "prebiotic chemistry." It informs our own suggestion that experimentation should look to the kind of nanoengines that must have been the precursors to molecular motors-such as pyrophosphate synthetase and the like driven by these gradients-that make life work. It is these putative free energy or disequilibria converters, presumably constructed from minerals comprising the earliest inorganic membranes, that, as obstacles to vectorial ionic flows, present themselves as the candidates for future experiments. Key Words: Methanotrophy-Origin of life. Astrobiology 14, 308-343.
C1 [Russell, Michael J.; Barge, Laura M.; Bhartia, Rohit; Kidd, Richard; Meier, David H.; Vance, Steve; White, Lauren; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bocanegra, Dylan] Art Ctr Bridge, Pasadena, CA USA.
[Bracher, Paul J.] CALTECH, Beckman Inst, Pasadena, CA 91109 USA.
[Bracher, Paul J.] St Louis Univ, Dept Chem, St Louis, MO 63103 USA.
[Branscomb, Elbert] UIUC, Inst Genom Biol, Champaign, IL USA.
[McGlynn, Shawn] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91109 USA.
[Nitschke, Wolfgang] CNRS, Bioenerget & Ingn Prot UPR9036, IFR88, Marseille, France.
[Shibuya, Takazo] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Precambrian Ecosyst Lab PEL, Yokosuka, Kanagawa, Japan.
[White, Lauren] Univ Calif Santa Barbara, Dept Chem & Biochem, Santa Barbara, CA 93106 USA.
RP Russell, MJ (reprint author), CALTECH, Jet Prop Lab, Chem & Astrobiol Sect 3225, MS 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mrussell@jpl.nasa.gov
OI Nitschke, Wolfgang/0000-0003-2084-3032; Bracher,
Paul/0000-0001-5769-8364
FU National Aeronautics and Space Administration; NASA Exobiology and
Evolutionary Biology award [NNH06ZDA001N]; NASA Astrobiology Institute
(Icy Worlds); NASA Astrobiology Institute (Universal Biology)
FX We thank John Allen, Ariel Anbar, Jean Bedard, Billy Brazelton, John
Callas, Ivria Doloboff, Kevin Hand, Mickey Honchell, Michael Malaska,
Randall Mielke, Ken Nealson, Yuk Yung, and the Thermodynamics,
Disequilibrium and Evolution (TDE) NAI Focus Group for discussions, and
two anonymous reviewers for their suggestions. The research described in
this publication was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration, with support by a NASA Exobiology
and Evolutionary Biology award (NNH06ZDA001N) and supported by the NASA
Astrobiology Institute (Icy Worlds). E.B. is supported by the NASA
Astrobiology Institute (Universal Biology).
NR 476
TC 43
Z9 44
U1 22
U2 156
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 APR 1
PY 2014
VL 14
IS 4
BP 308
EP 343
DI 10.1089/ast.2013.1110
PG 36
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA AF0UX
UT WOS:000334430700004
PM 24697642
ER
PT J
AU McKay, CP
Anbar, AD
Porco, C
Tsou, P
AF McKay, Christopher P.
Anbar, Ariel D.
Porco, Carolyn
Tsou, Peter
TI Follow the Plume: The Habitability of Enceladus
SO ASTROBIOLOGY
LA English
DT Article
ID SOUTH-POLE; LIFE; ORIGIN; SEARCH; MARS; METHANE; WATER
AB The astrobiological exploration of other worlds in our Solar System is moving from initial exploration to more focused astrobiology missions. In this context, we present the case that the plume of Enceladus currently represents the best astrobiology target in the Solar System. Analysis of the plume by the Cassini mission indicates that the steady plume derives from a subsurface liquid water reservoir that contains organic carbon, biologically available nitrogen, redox energy sources, and inorganic salts. Furthermore, samples from the plume jetting out into space are accessible to a low-cost flyby mission. No other world has such well-studied indications of habitable conditions. Thus, the science goals that would motivate an Enceladus mission are more advanced than for any other Solar System body. The goals of such a mission must go beyond further geophysical characterization, extending to the search for biomolecular evidence of life in the organic-rich plume. This will require improved in situ investigations and a sample return. Key Words: Ice-Life detection-Icy moon. Astrobiology 14, 352-355.
C1 [McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Anbar, Ariel D.] Arizona State Univ, Tempe, AZ USA.
[Porco, Carolyn] Space Sci Inst, CICLOPS, Boulder, CO USA.
[Tsou, Peter] Sample Explorat Syst, La Canada Flintridge, CA USA.
RP McKay, CP (reprint author), NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM chris.mckay@nasa.gov
NR 27
TC 12
Z9 12
U1 7
U2 66
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 APR 1
PY 2014
VL 14
IS 4
BP 352
EP 355
DI 10.1089/ast.2014.1158
PG 4
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA AF0UX
UT WOS:000334430700006
PM 24684187
ER
PT J
AU Akrami, Y
Fantaye, Y
Shafieloo, A
Eriksen, HK
Hansen, FK
Banday, AJ
Gorski, KM
AF Akrami, Y.
Fantaye, Y.
Shafieloo, A.
Eriksen, H. K.
Hansen, F. K.
Banday, A. J.
Gorski, K. M.
TI POWER ASYMMETRY IN WMAP AND PLANCK TEMPERATURE SKY MAPS AS MEASURED BY A
LOCAL VARIANCE ESTIMATOR
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmic background radiation; cosmology: observations; methods:
statistical
ID MICROWAVE-ANISOTROPY-PROBE; DIRECTIONAL SPHERICAL WAVELETS; BACKGROUND
ANISOTROPY; NON-GAUSSIANITY; VIIH MODELS; ANOMALIES; ISOTROPY; UNIVERSE;
FIELD
AB We revisit the question of hemispherical power asymmetry in the WMAP and Planck temperature sky maps by measuring the local variance over the sky and on disks of various sizes. For the 2013 Planck sky map we find that none of the 1000 available isotropic Planck "Full Focal Plane" simulations have a larger variance asymmetry than that estimated from the data, suggesting the presence of an anisotropic signature formally significant at least at the 3.3 sigma level. For the WMAP 9 year data we find that 5 out of 1000 simulations have a larger asymmetry. The preferred direction for the asymmetry from the Planck data is (l, b) = (212 degrees, -13 degrees), in good agreement with previous reports of the same hemispherical power asymmetry.
C1 [Akrami, Y.; Fantaye, Y.; Eriksen, H. K.; Hansen, F. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Fantaye, Y.] Univ Roma Tor Vergata, Dept Math, Rome, Italy.
[Shafieloo, A.] Asia Pacific Ctr Theoret Phys, Pohang 790784, Gyeongbuk, South Korea.
[Shafieloo, A.] POSTECH, Dept Phys, Pohang 790784, Gyeongbuk, South Korea.
[Banday, A. J.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Banday, A. J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Gorski, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Akrami, Y (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, N-0315 Oslo, Norway.
EM yashar.akrami@astro.uio.no; y.t.fantaye@astro.uio.no; arman@apctp.org
OI Akrami, Yashar/0000-0002-2407-7956
FU ERC Starting Grant [StG2010-257080]; ERC [277742 Pascal]; Korean
Ministry of Education, Science and Technology (MEST); Gyeongsangbuk-Do;
Pohang City; National Research Foundation of Korea
[NRF-2013R1A1A2013795]; OYI grant from the Norwegian research council
FX We thank Claudio Llinares, Eamon M. Scullion, and Amir Hajian for
helpful discussions. Y.A. and H.K.E. acknowledge support through the ERC
Starting Grant StG2010-257080. Y.F. is supported by ERC Grant 277742
Pascal. A.S. thanks the Korean Ministry of Education, Science and
Technology (MEST), Gyeongsangbuk-Do, and Pohang City for the support of
the Independent Junior Research Groups at the Asia Pacific Center for
Theoretical Physics (APCTP). A.S. would like to acknowledge the support
of the National Research Foundation of Korea (NRF-2013R1A1A2013795).
F.K.H. acknowledges OYI grant from the Norwegian research council. 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).
NR 51
TC 69
Z9 69
U1 1
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 1
PY 2014
VL 784
IS 2
AR L42
DI 10.1088/2041-8205/784/2/L42
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AD5ZX
UT WOS:000333333400025
ER
PT J
AU Bellm, EC
Barriere, NM
Bhalerao, V
Boggs, SE
Cenko, SB
Christensen, FE
Craig, WW
Forster, K
Fryer, CL
Hailey, CJ
Harrison, FA
Horesh, A
Kouveliotou, C
Madsen, KK
Miller, JM
Ofek, EO
Perley, DA
Rana, VR
Reynolds, SP
Stern, D
Tomsick, JA
Zhang, WW
AF Bellm, Eric C.
Barriere, Nicolas M.
Bhalerao, Varun
Boggs, Steven E.
Cenko, S. Bradley
Christensen, Finn E.
Craig, William W.
Forster, Karl
Fryer, Chris L.
Hailey, Charles J.
Harrison, Fiona A.
Horesh, Assaf
Kouveliotou, Chryssa
Madsen, Kristin K.
Miller, Jon M.
Ofek, Eran O.
Perley, Daniel A.
Rana, Vikram R.
Reynolds, Stephen P.
Stern, Daniel
Tomsick, John A.
Zhang, William W.
TI X-RAY SPECTRAL COMPONENTS OBSERVED IN THE AFTERGLOW OF GRB 130925A
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE gamma-ray burst: individual (GRB 130925A)
ID MASSIVE BLACK-HOLE; SUPERNOVA; BURSTS; STAR; EMISSION; SEARCH;
SIGNATURES; COLLAPSARS; ACCRETION; OUTBURST
AB We have identified spectral features in the late-time X-ray afterglow of the unusually long, slow-decaying GRB 130925A using NuSTAR, Swift/X-Ray Telescope, and Chandra. A spectral component in addition to an absorbed power law is required at >4 sigma significance, and its spectral shape varies between two observation epochs at 2 x 10(5) and 10(6) s after the burst. Several models can fit this additional component, each with very different physical implications. A broad, resolved Gaussian absorption feature of several keV width improves the fit, but it is poorly constrained in the second epoch. An additive blackbody or second power-law component provide better fits. Both are challenging to interpret: the blackbody radius is near the scale of a compact remnant (10(8) cm), while the second power-law component requires an unobserved high-energy cutoff in order to be consistent with the non-detection by Fermi/Large Area Telescope.
C1 [Bellm, Eric C.; Forster, Karl; Harrison, Fiona A.; Madsen, Kristin K.; Perley, Daniel A.; Rana, Vikram R.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Barriere, Nicolas M.; Boggs, Steven E.; Craig, William W.; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bhalerao, Varun] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Cenko, S. Bradley; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Fryer, Chris L.] Los Alamos Natl Lab, CCS 2, Los Alamos, NM 87545 USA.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Horesh, Assaf; Ofek, Eran O.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Astrophys Off ZP12, Huntsville, AL 35812 USA.
[Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Reynolds, Stephen P.] NC State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bellm, EC (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
EM ebellm@caltech.edu
RI Boggs, Steven/E-4170-2015; Horesh, Assaf/O-9873-2016;
OI Boggs, Steven/0000-0001-9567-4224; Horesh, Assaf/0000-0002-5936-1156;
Bhalerao, Varun/0000-0002-6112-7609; Madsen,
Kristin/0000-0003-1252-4891; Rana, Vikram/0000-0003-1703-8796
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration
FX This work was supported under NASA contract No. NNG08FD60C and uses 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 team for executing the target of opportunity observations.
This research has used the NuSTAR Data Analysis Software (NuSTARDAS)
jointly developed by the ASI Science Data Center (ASDC, Italy) and the
California Institute of Technology (USA). These results are based in
part on observations made by the Chandra X-ray Observatory. We thank the
Chandra director for granting discretionary time and the Chandra team
for prompt execution of the observations.
NR 47
TC 10
Z9 10
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 1
PY 2014
VL 784
IS 2
AR L19
DI 10.1088/2041-8205/784/2/L19
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AD5ZX
UT WOS:000333333400002
ER
PT J
AU Burgess, JM
Preece, RD
Ryde, F
Veres, P
Meszaros, P
Connaughton, V
Briggs, M
Pe'er, A
Iyyani, S
Goldstein, A
Axelsson, M
Baring, MG
Bhat, PN
Byrne, D
Fitzpatrick, G
Foley, S
Kocevski, D
Omodei, N
Paciesas, WS
Pelassa, V
Kouveliotou, C
Xiong, SL
Yu, HF
Zhang, BB
Zhu, S
AF Burgess, J. Michael
Preece, Robert D.
Ryde, Felix
Veres, Peter
Meszaros, Peter
Connaughton, Valerie
Briggs, Michael
Pe'er, Asaf
Iyyani, Shabnam
Goldstein, Adam
Axelsson, Magnus
Baring, Matthew G.
Bhat, P. N.
Byrne, David
Fitzpatrick, Gerard
Foley, Suzanne
Kocevski, Daniel
Omodei, Nicola
Paciesas, William S.
Pelassa, Veronique
Kouveliotou, Chryssa
Xiong, Shaolin
Yu, Hoi-Fung
Zhang, Binbin
Zhu, Sylvia
TI AN OBSERVED CORRELATION BETWEEN THERMAL AND NON-THERMAL EMISSION IN
GAMMA-RAY BURSTS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE gamma-ray burst: general; radiation mechanisms: non-thermal; radiation
mechanisms: thermal
ID FERMI-LAT OBSERVATIONS; PHOTOSPHERIC EMISSION; SPECTRAL CATALOG; PROMPT
EMISSION; GRB OUTFLOWS; MODEL; DISSIPATION; EFFICIENCY; ACCELERATION;
RECONNECTION
AB Recent observations by the Fermi Gamma-ray Space Telescope have confirmed the existence of thermal and non-thermal components in the prompt photon spectra of some gamma-ray bursts (GRBs). Through an analysis of six bright Fermi GRBs, we have discovered a correlation between the observed photospheric and non-thermal gamma-ray emission components of several GRBs using a physical model that has previously been shown to be a good fit to the Fermi data. From the spectral parameters of these fits we find that the characteristic energies, E-p and kT, of these two components are correlated via the relation E-p proportional to T-alpha which varies from GRB to GRB. We present an interpretation in which the value of the index alpha indicates whether the jet is dominated by kinetic or magnetic energy. To date, this jet composition parameter has been assumed in the modeling of GRB outflows rather than derived from the data.
C1 [Burgess, J. Michael; Preece, Robert D.] Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA.
[Burgess, J. Michael; Preece, Robert D.; Connaughton, Valerie; Briggs, Michael; Bhat, P. N.; Pelassa, Veronique; Xiong, Shaolin; Zhang, Binbin] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Burgess, J. Michael; Ryde, Felix; Iyyani, Shabnam; Axelsson, Magnus] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Ryde, Felix; Iyyani, Shabnam; Axelsson, Magnus] AlbaNova, Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Veres, Peter; Meszaros, Peter] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Pe'er, Asaf] Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland.
[Iyyani, Shabnam; Kouveliotou, Chryssa] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
[Goldstein, Adam] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Axelsson, Magnus] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Baring, Matthew G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Byrne, David; Fitzpatrick, Gerard; Foley, Suzanne] Univ Coll Dublin, Dublin 4, Ireland.
[Foley, Suzanne; Yu, Hoi-Fung] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kocevski, Daniel; Omodei, Nicola] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Kocevski, Daniel; Omodei, Nicola] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Paciesas, William S.] Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Zhu, Sylvia] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Zhu, Sylvia] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Burgess, JM (reprint author), Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA.
EM jmichaelburgess@gmail.com; rob.preece@nasa.gov; felix@particle.kth.se;
veres@gwu.edu; npp@astro.psu.edu
RI Zhang, Binbin/C-9035-2013; Iyyani, Shabnam/D-8736-2017;
OI Zhang, Binbin/0000-0003-2002-116X; Iyyani, Shabnam/0000-0002-2525-3464;
Preece, Robert/0000-0003-1626-7335; Burgess, James/0000-0003-3345-9515;
Veres, Peter/0000-0002-2149-9846; Axelsson, Magnus/0000-0003-4378-8785
NR 47
TC 14
Z9 14
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 APR 1
PY 2014
VL 784
IS 2
AR L43
DI 10.1088/2041-8205/784/2/L43
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AD5ZX
UT WOS:000333333400026
ER
PT J
AU Furst, F
Pottschmidt, K
Wilms, J
Kennea, J
Bachetti, M
Bellm, E
Boggs, SE
Chakrabarty, D
Christensen, FE
Craig, WW
Hailey, CJ
Harrison, F
Stern, D
Tomsick, JA
Walton, DJ
Zhang, W
AF Fuerst, Felix
Pottschmidt, Katja
Wilms, Joern
Kennea, Jamie
Bachetti, Matteo
Bellm, Eric
Boggs, Steven E.
Chakrabarty, Deepto
Christensen, Finn E.
Craig, William W.
Hailey, Charles J.
Harrison, Fiona
Stern, Daniel
Tomsick, John A.
Walton, Dominic J.
Zhang, William
TI NuSTAR DISCOVERY OF A CYCLOTRON LINE IN KS 1947+300
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; radiation: dynamics; stars: neutron; X-rays:
binaries; X-rays: individual (KS 1947+300)
ID X-RAY; COMPTONIZATION MODELS; INTERSTELLAR-MEDIUM; SPECTROSCOPY;
KS-1947+300; ENERGY; TELESCOPE; PULSARS; MISSION; RXTE
AB We present a spectral analysis of three simultaneous Nuclear Spectroscopy Telescope Array and Swift/XRT observations of the transient Be-neutron star binary KS 1947+300 taken during its outburst in 2013/2014. These broadband observations were supported by Swift/XRT monitoring snapshots every three days, which we use to study the evolution of the spectrum over the outburst. We find strong changes of the power-law photon index, which shows a weak trend of softening with increasing X-ray flux. The neutron star shows very strong pulsations with a period of P approximate to 18.8 s. The 0.8-79 keV broadband spectrum can be described by a power law with an exponential cutoff and a blackbody component at low energies. During the second observation we detect a cyclotron resonant scattering feature at 12.5 keV, which is absent in the phase-averaged spectra of observations 1 and 3. Pulse phase-resolved spectroscopy reveals that the strength of the feature changes strongly with pulse phase and is most prominent during the broad minimum of the pulse profile. At the same phases the line also becomes visible in the first and third observation at the same energy. This discovery implies that KS 1947+300 has a magnetic field strength of B approximate to 1.1 x 10(12)(1 + z) G, which is at the lower end of known cyclotron line sources.
C1 [Fuerst, Felix; Bellm, Eric; Harrison, Fiona; Walton, Dominic J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Pottschmidt, Katja] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Pottschmidt, Katja] CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Wilms, Joern] Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany.
[Wilms, Joern] ECAP, D-96049 Bamberg, Germany.
[Kennea, Jamie] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Bachetti, Matteo] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France.
[Bachetti, Matteo] CNRS, Inst Rech Astrophys & Planetol, 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.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, William] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Furst, F (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RI Wilms, Joern/C-8116-2013; Boggs, Steven/E-4170-2015;
OI Wilms, Joern/0000-0003-2065-5410; Boggs, Steven/0000-0001-9567-4224;
Bellm, Eric/0000-0001-8018-5348; Bachetti, Matteo/0000-0002-4576-9337
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
Deutsches Zentrum fur Luft-und Raumfahrt under DLR grant [50 OR 1113]
FX We would like to thank Matthias Kuhnel, Ralf Ballhausen, Fritz Schwarm,
and Peter Kretschmar for useful discussions. 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). This research has made use of ISIS functions provided by
ECAP/Remeis observatory and MIT
(http://www.sternwarte.uni-erlangen.de/isis/). We thank the Deutsches
Zentrum fur Luft-und Raumfahrt for partial support under DLR grant 50 OR
1113. We thank the anonymous referee for useful comments.
NR 32
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U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 1
PY 2014
VL 784
IS 2
AR L40
DI 10.1088/2041-8205/784/2/L40
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AD5ZX
UT WOS:000333333400023
ER
PT J
AU Yang, B
Keane, J
Meech, K
Owen, T
Wainscoat, R
AF Yang, Bin
Keane, Jacqueline
Meech, Karen
Owen, Tobias
Wainscoat, Richard
TI MULTI-WAVELENGTH OBSERVATIONS OF COMET C/2011 L4 (PAN-STARRS)
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE comets: individual (C/2011 L4); infrared: planetary systems; Oort Cloud
ID DUST RELEASE RATES; HALE-BOPP; WATER ICE; MU-M; GAS; GRAINS;
SPECTROGRAPH; OUTBURSTS; DISTANCE; NUCLEI
AB The dynamically new comet C/2011 L4 (Pan-STARRS) is one of the brightest comets observed since the great comet C/1995 O1 (Hale-Bopp). Here, we present our multi-wavelength observations of C/2011 L4 during its in-bound passage to the inner solar system. A strong absorption band of water ice at 2.0 mu m was detected in the near-infrared spectra, obtained with the 8 m Gemini-North and 3 m Infrared Telescope Facility Telescopes. The companion 1.5 mu m band of water ice, however, was not observed. Spectral modeling shows that the absence of the 1.5 mu m feature can be explained by the presence of sub-micron-sized fine ice grains. No gas lines (i.e., CN, HCN, or CO) were observed pre-perihelion in either the optical or the submillimeter. We derived 3 sigma upper limits for the CN and CO production rates. The comet exhibited a very strong continuum in the optical and its slope seemed to become redder as the comet approached the Sun. Our observations suggest that C/2011 L4 is an unusually dust-rich comet with a dust-to-gas mass ratio >4.
C1 [Yang, Bin; Keane, Jacqueline; Meech, Karen] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
[Yang, Bin] European So Observ, Santiago 19, Chile.
[Meech, Karen; Owen, Tobias; Wainscoat, Richard] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Yang, B (reprint author), Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
EM yangbin@ifa.hawaii.edu
FU NASA Astrobiology Institute through the Office of Space Science
[NNA08DA77A]; NSF [AST-1010059]
FX We thank Jason X. Prochaska and Kate Rubin for helping us with the GMOS
data reduction and Zahed Wahhaj and David Jewitt for valuable
discussions and constructive suggestions. We thank the JCMT staff for
their assistance. B.Y. was supported by the NASA Astrobiology Institute
under Cooperative Agreement No. NNA08DA77A issued through the Office of
Space Science. Work was supported in part by NSF grant AST-1010059.
NR 49
TC 8
Z9 8
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 1
PY 2014
VL 784
IS 2
AR L23
DI 10.1088/2041-8205/784/2/L23
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AD5ZX
UT WOS:000333333400006
ER
PT J
AU Chen, CH
Mittal, T
Kuchner, M
Forrest, WJ
Lisse, CM
Manoj, P
Sargent, BA
Watson, DM
AF Chen, Christine H.
Mittal, Tushar
Kuchner, Marc
Forrest, William J.
Lisse, Carey M.
Manoj, P.
Sargent, Benjamin A.
Watson, Dan M.
TI THE SPITZER INFRARED SPECTROGRAPH DEBRIS DISK CATALOG. I. CONTINUUM
ANALYSIS OF UNRESOLVED TARGETS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; circumstellar matter; infrared: stars; zodiacal dust
ID MAIN-SEQUENCE STARS; M-CIRCLE-DOT; SOLAR-TYPE STARS; LOW-MASS STARS;
T-TAURI STARS; A-TYPE STARS; STELLAR KINEMATIC GROUPS; PICTORIS MOVING
GROUP; SUN-LIKE STARS; MULTIBAND IMAGING PHOTOMETER
AB During the Spitzer Space Telescope cryogenic mission, Guaranteed Time Observers, Legacy Teams, and General Observers obtained Infrared Spectrograph (IRS) observations of hundreds of debris disk candidates. We calibrated the spectra of 571 candidates, including 64 new IRAS and Multiband Imaging Photometer for Spitzer (MIPS) debris disks candidates, modeled their stellar photospheres, and produced a catalog of excess spectra for unresolved debris disks. For 499 targets with IRS excess but without strong spectral features (and a subset of 420 targets with additional MIPS 70 mu m observations), we modeled the IRS (and MIPS data) assuming that the dust thermal emission was well-described using either a one- or two-temperature blackbody model. We calculated the probability for each model and computed the average probability to select among models. We found that the spectral energy distributions for the majority of objects (similar to 66%) were better described using a two-temperature model with warm (T-gr similar to 100-500 K) and cold (T-gr similar to 50-150 K) dust populations analogous to zodiacal and Kuiper Belt dust, suggesting that planetary systems are common in debris disks and zodiacal dust is common around host stars with ages up to similar to 1 Gyr. We found that younger stars generally have disks with larger fractional infrared luminosities and higher grain temperatures and that higher-mass stars have disks with higher grain temperatures. We show that the increasing distance of dust around debris disks is inconsistent with self-stirred disk models, expected if these systems possess planets at 30-150 AU. Finally, we illustrate how observations of debris disks may be used to constrain the radial dependence of material in the minimum mass solar nebula.
C1 [Chen, Christine H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Mittal, Tushar] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Kuchner, Marc] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Forrest, William J.; Watson, Dan M.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Manoj, P.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Sargent, Benjamin A.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
[Sargent, Benjamin A.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA.
RP Chen, CH (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM cchen@stsci.edu
RI Lisse, Carey/B-7772-2016
OI Lisse, Carey/0000-0002-9548-1526
FU STScI Director's Discretionary Fund; NASA; NSF; JPL/Caltech
FX We would like to thank Chas Beichman, Mike Fitzgerald, Laura Hanley,
Hannah Jang-Condell, Margaret Moerchen, our referee (Farisa Morales),
and our editor (Eric Feigelson) for their helpful comments and
suggestions. This work is based on observations made with the Spitzer
Space Telescope, which is operated by JPL/Caltech under a contract with
NASA. Support for this work was provided by NASA through an award issued
by JPL/Caltech and by the STScI Director's Discretionary Fund. This
research made use of the SIMBAD database, operated at CDS, Strasbourg,
France, and data products from the 2MASS, which is a joint project of
the University of Massachusetts and the Infrared Processing and Analysis
Center/Caltech, funded by NASA and the NSF.
NR 192
TC 61
Z9 61
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD APR
PY 2014
VL 211
IS 2
AR 25
DI 10.1088/0067-0049/211/2/25
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE5KT
UT WOS:000334028600009
ER
PT J
AU Heays, AN
Ajello, JM
Aguilar, A
Lewis, BR
Gibson, ST
AF Heays, A. N.
Ajello, J. M.
Aguilar, A.
Lewis, B. R.
Gibson, S. T.
TI THE HIGH-RESOLUTION EXTREME-ULTRAVIOLET SPECTRUM OF N-2 BY ELECTRON
IMPACT
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE line: identification; minor planets, asteroids: individual (Titan);
molecular data; planets and satellites: atmospheres; radiation
mechanisms: non-thermal; ultraviolet: general
ID VUV ABSORPTION-SPECTRUM; EMISSION CROSS-SECTION; MOLECULAR NITROGEN;
DIATOMIC-MOLECULES; RYDBERG STATES; DISSOCIATIVE EXCITATION;
SCATTERING-THEORY; EXCITED-STATES; PREDISSOCIATION; SPECTROSCOPY
AB We have analyzed high-resolution (FWHM = 0.2 angstrom) extreme-ultraviolet (EUV, 800-1350 angstrom) laboratory emission spectra of molecular nitrogen excited by an electron impact at 20 and 100 eV under (mostly) optically thin, single-scattering experimental conditions. A total of 491 emission features were observed from N-2 electronic-vibrational transitions and atomic Ni and NII multiplets and their emission cross sections were measured. Molecular emission was observed at vibrationally excited ground-state levels as high as v '' = 17, from the a(1)Pi(g), b(1)Pi(u), and b '(1)Sigma(+)(u) excited valence states and the Rydberg series c '(n+1) (1)Sigma u(+), c(n) (1)Pi(u), and O-n (1)Pi(u) for n between 3 and 9. The frequently blended molecular emission bands were disentangled with the aid of a sophisticated and predictive quantum-mechanical model of excited states that includes the strong coupling between valence and Rydberg electronic states and the effects of predissociation. Improved model parameters describing electronic transition moments were obtained from the experiment and allowed for a reliable prediction of the vibrationally summed electronic emission cross section, including an extrapolation to unobserved emission bands and those that are optically thick in the experimental spectra. Vibrationally dependent electronic excitation functions were inferred from a comparison of emission features following 20 and 100 eV electron-impact collisional excitation. The electron-impact-induced fluorescence measurements are compared with Cassini Ultraviolet Imaging Spectrograph observations of emissions from Titan's upper atmosphere.
C1 [Heays, A. N.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Heays, A. N.; Lewis, B. R.; Gibson, S. T.] Australian Natl Univ, Res Sch Phys & Engn, Canberra, ACT 0200, Australia.
[Ajello, J. M.; Aguilar, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Heays, AN (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM heays@strw.leidenuniv.nl
OI Heays, Alan/0000-0002-7716-9192
FU National Aeronautics and Space Administration (NASA); NASA's Cassini
Data Analysis Program; Geospace program; National Science Foundation;
Astronomy and Physics Research and Analysis Program; Space Physics
Program Offices; Australian Research Council Discovery Program
[DP0558962, DP0773050]; Netherlands Organisation for Scientific Research
(NWO) [648.000.002]; Planetary Atmospheres program
FX This work was performed at the Jet Propulsion Laboratory (JPL),
California Institute of Technology (Caltech), under a contract with the
National Aeronautics and Space Administration (NASA). We gratefully
acknowledge financial support through NASA's Cassini Data Analysis
Program, Geospace and Planetary Atmospheres programs, the National
Science Foundation, the Astronomy and Physics Research and Analysis
Program, and Space Physics Program Offices. Calculations of the
N2 photodissociation cross sections were supported by the
Australian Research Council Discovery Program, through grant Nos.
DP0558962 and DP0773050. A. H. was supported by grant number 648.000.002
from the Netherlands Organisation for Scientific Research (NWO) via the
Dutch Astrochemistry Network.
NR 101
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U1 1
U2 25
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD APR
PY 2014
VL 211
IS 2
DI 10.1088/0067-0049/211/2/28
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AE5KT
UT WOS:000334028600012
ER
PT J
AU Subramanian, A
Jochum, M
Miller, AJ
Neale, R
Seo, H
Waliser, D
Murtugudde, R
AF Subramanian, Aneesh
Jochum, Markus
Miller, Arthur J.
Neale, Richard
Seo, Hyodae
Waliser, Duane
Murtugudde, Raghu
TI The MJO and global warming: a study in CCSM4
SO CLIMATE DYNAMICS
LA English
DT Article
DE MJO; Climate change; CCSM4
ID MADDEN-JULIAN OSCILLATION; PRECIPITATION EXTREMES; ATMOSPHERIC
CIRCULATION; EQUATORIAL PACIFIC; HYDROLOGICAL CYCLE; CLIMATE-CHANGE;
IDEALIZED GCM; WIDE-RANGE; EL-NINO; ENSO
AB The change in Madden-Julian oscillation (MJO) amplitude and variance in response to anthropogenic climate change is assessed in the 1A degrees nominal resolution community climate system model, version 4 (CCSM4), which has a reasonable representation of the MJO characteristics both dynamically and statistically. The twentieth century CCSM4 run is compared with the warmest twenty-first century projection (representative concentration pathway 8.5, or RCP8.5). The last 20 years of each simulation are compared in their MJO characteristics, including spatial variance distributions of winds, precipitation and outgoing longwave radiation, histograms of event amplitude, phase and duration, and composite maps of phases. The RCP8.5 run exhibits increased variance in intraseasonal precipitation, larger-amplitude MJO events, stronger MJO rainfall in the central and eastern tropical Pacific, and a greater frequency of MJO occurrence for phases corresponding to enhanced rainfall in the Indian Ocean sector. These features are consistent with the concept of an increased magnitude for the hydrological cycle under greenhouse warming conditions. Conversely, the number of active MJO days decreases and fewer weak MJO events occur in the future climate state. These results motivate further study of these changes since tropical rainfall variability plays such an important role in the region's socio-economic well being.
C1 [Subramanian, Aneesh; Miller, Arthur J.] UCSD, SIO, La Jolla, CA 92037 USA.
[Jochum, Markus] Niels Bohr Inst, Climate & Geophys Div, DK-2100 Copenhagen, Denmark.
[Neale, Richard] Natl Ctr Atmospher Res, Climate & Global Dynam Div, Boulder, CO 80307 USA.
[Seo, Hyodae] Woods Hole Oceanog Inst, Dept Phys Oceanog, Woods Hole, MA 02543 USA.
[Waliser, Duane] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Murtugudde, Raghu] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Subramanian, A (reprint author), UCSD, SIO, La Jolla, CA 92037 USA.
EM acsubram@ucsd.edu
RI jochum, markus/C-2960-2015; Subramanian, Aneesh/D-9484-2017
OI jochum, markus/0000-0003-2690-3139; Subramanian,
Aneesh/0000-0001-7805-0102
FU ONR [N00014-13-1-0139]; NSF [OCE-0960770]; SUNNY (Scripps/UCSD/NCAR New
and Young) Program
FX This research forms a part of the Ph.D. dissertation of A.S. We
gratefully acknowledge funding from ONR (N00014-13-1-0139) and NSF
(OCE-0960770). This research was initiated during a visit by A.S. to
NCAR funded by the SUNNY (Scripps/UCSD/NCAR New and Young) Program. A.S.
acknowledges NCARs computational support for simulations conducted for
this study. We thank Mitch Moncrieff and Brian Mapes for erudite
comments, and criticism of this work. A.S. extends heartfelt thanks to
Bruce Cornuelle and Ian Eisenman for many invaluable gems of wisdom on
science and data analysis. 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 48
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U1 2
U2 32
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD APR
PY 2014
VL 42
IS 7-8
BP 2019
EP 2031
DI 10.1007/s00382-013-1846-1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AE5ZP
UT WOS:000334068100019
ER
PT J
AU Dushaw, BD
Menemenlis, D
AF Dushaw, Brian D.
Menemenlis, Dimitris
TI Antipodal acoustic thermometry: 1960, 2004
SO DEEP-SEA RESEARCH PART I-OCEANOGRAPHIC RESEARCH PAPERS
LA English
DT Article
DE Antipodal acoustics; Ocean modeling; Acoustic tomography; Climate change
ID NORTH PACIFIC-OCEAN; HEARD ISLAND; HYDROACOUSTIC SIGNALS; UNDERWATER
EXPLOSIONS; GENERAL-CIRCULATION; SOUND-TRANSMISSION; RANGE; BERMUDA;
SPEED; AUSTRALIA
AB On 21 March 1960, sounds from three 300-lb depth charges deployed at 5.5-min intervals off Perth, Australia were recorded by the SOFAR station at Bermuda. The recorded travel time of these signals, about 13,375 s, is a historical measure of the ocean temperature averaged across several ocean basins. The 1960 travel time measurement has about 3-s precision. High-resolution global ocean state estimates for 2004 from the "Estimating the Circulation and Climate of the Ocean, Phase II" (ECCO2) project were combined with ray tracing to determine the paths followed by the acoustic signals. The acoustic paths are refracted geodesics that are slightly deflected by either small-scale topographic features in the Southern Ocean or the coast of Brazil. The refractive influences of intense, small-scale oceanographic features, such as Agulhas Rings or eddies in the Antarctic Circumpolar Current, greatly reduce the necessary topographic deflection and cause the acoustic paths to meander in time. The ECCO2 ocean state estimates, which are constrained by model dynamics and available data, were used to compute present-day travel times. Measured and computed arrival coda were in good agreement. Based on recent estimates of warming of the upper ocean, the travel-time change over the past half-century was nominally expected to be about -9 s, but little difference between measured (1960) and computed (2004) travel times was found. Taking into account uncertainties in the 1960 measurements, the 2004 ocean state estimates, and other approximations, the ocean temperature averaged along the sound channel axis over the antipodal paths has warmed at a rate less than about 4.6 m degrees C yr(-1) (95% confidence). At this time, the estimated uncertainties are comparable in size to the expected warming signal, however. (C) 2014 The Authors. Published by Elsevier Ltd. All rights reserved.
C1 [Dushaw, Brian D.] Univ Washington, Appl Phys Lab, Seattle, WA 98105 USA.
[Menemenlis, Dimitris] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Dushaw, BD (reprint author), Univ Washington, Appl Phys Lab, 1013 NE 40th St, Seattle, WA 98105 USA.
EM dushaw@apl.washington.edu
OI Menemenlis, Dimitris/0000-0001-9940-8409
FU National Science Foundation [OCE-0850357]; Office of Naval Research
[N00014-09-1-0446, N00014-12-1-0183]
FX This project was supported by National Science Foundation Grant
OCE-0850357 and Office of Naval Research Grants N00014-09-1-0446,
N00014-12-1-0183. D.M. 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. Thanks are due to Lieutenant Commander Ian
Jempson RAN (Navigating Officer, ret.) of the Queensland Maritime Museum
for providing essential assistance in the interpretation of the HMAS
Diamantina Ship's Log and other information. We would like to thank the
staffs of the National Archives of Australia and the Australian War
Memorial for their helpful efficiency in locating and making available
material related to HMAS Diamantina and the 1960 experiment.
NR 64
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U1 0
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0637
EI 1879-0119
J9 DEEP-SEA RES PT I
JI Deep-Sea Res. Part I-Oceanogr. Res. Pap.
PD APR
PY 2014
VL 86
BP 1
EP 20
DI 10.1016/j.dsr.2013.12.008
PG 20
WC Oceanography
SC Oceanography
GA AE8MR
UT WOS:000334256500001
ER
PT J
AU Kavaya, MJ
Beyon, JY
Koch, GJ
Petros, M
Petzar, PJ
Singh, UN
Trieu, BC
Yu, JR
AF Kavaya, Michael J.
Beyon, Jeffrey Y.
Koch, Grady J.
Petros, Mulugeta
Petzar, Paul J.
Singh, Upendra N.
Trieu, Bo C.
Yu, Jirong
TI The Doppler Aerosol Wind (DAWN) Airborne, Wind-Profiling
Coherent-Detection Lidar System: Overview and Preliminary Flight Results
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
DE Lidars/Lidar observations; Aircraft observations; Remote sensing; Wind
profilers; Profilers, atmospheric
ID LASER-RADAR; PERFORMANCE; EFFICIENCY; ERROR; SPACE
AB The first airborne wind measurements of a pulsed, 2-mu m solid-state, high-energy, wind-profiling lidar system for airborne measurements are presented. The laser pulse energy is the highest to date in an eye-safe airborne wind lidar system. This energy, the 10-Hz laser pulse rate, the 15-cm receiver diameter, and dual-balanced coherent detection together have the potential to provide much-improved lidar sensitivity to low aerosol backscatter levels compared to earlier airborne-pulsed coherent lidar wind systems. Problems with a laser-burned telescope secondary mirror prevented a full demonstration of the lidar's capability, but the hardware, algorithms, and software were nevertheless all validated. A lidar description, relevant theory, and preliminary results of flight measurements are presented.
C1 [Kavaya, Michael J.; Beyon, Jeffrey Y.; Koch, Grady J.; Petros, Mulugeta; Petzar, Paul J.; Singh, Upendra N.; Trieu, Bo C.; Yu, Jirong] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Kavaya, MJ (reprint author), NASA, Langley Res Ctr, 5 N Dryden St,Mail Code 468, Hampton, VA 23681 USA.
EM michael.j.kavaya@nasa.gov
FU NASA Science Mission Directorate, Earth Science Division, Earth Science
Technology Office; NASA Science Mission Directorate, Earth Science
Division; NASA Langley Research Center; NASA Langley Research Center,
Engineering Directorate; NASA Langley Research Center, Chief Engineer's
office
FX The authors acknowledge support from NASA Science Mission Directorate,
Earth Science Division, Earth Science Technology Office; NASA Science
Mission Directorate, Earth Science Division; NASA Langley Research
Center; NASA Langley Research Center, Engineering Directorate; and NASA
Langley Research Center, Chief Engineer's office.
NR 35
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U1 2
U2 23
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 APR
PY 2014
VL 31
IS 4
BP 826
EP 842
DI 10.1175/JTECH-D-12-00274.1
PG 17
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA AE6XX
UT WOS:000334142400005
ER
EF