FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Funsten, HO
Harper, RW
Dors, EE
Janzen, PA
Larsen, BA
MacDonald, EA
Poston, DI
Ritzau, SM
Skoug, RM
Zurbuchen, TH
AF Funsten, Herbert O.
Harper, Ronnie W.
Dors, Eric E.
Janzen, Paul A.
Larsen, Brian A.
MacDonald, Elizabeth A.
Poston, David I.
Ritzau, Stephen M.
Skoug, Ruth M.
Zurbuchen, Thomas H.
TI Comparative Response of Microchannel Plate and Channel Electron
Multiplier Detectors to Penetrating Radiation in Space
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE Electron multipliers; gamma-ray effects; plasma measurements; radiation
effects
ID X-RAY; EFFICIENCY; PROTONS; MODEL; FATIGUE
AB Channel electron multiplier (CEM) and microchannel plate (MCP) detectors are routinely used in space instrumentation for measurement of space plasmas. Our goal is to understand the relative sensitivities of these detectors to penetrating radiation in space, which can generate background counts and shorten detector lifetime. We use 662 keV gamma-rays as a proxy for penetrating radiation such as gamma-rays, cosmic rays, and high-energy electrons and protons that are ubiquitous in the space environment. We find that MCP detectors are similar to 20 times more sensitive to 662 keV gamma-rays than CEM detectors. This is attributed to the larger total area of multiplication channels in an MCP detector that is sensitive to electronic excitation and ionization resulting from the interaction of penetrating radiation with the detector material. In contrast to the CEM detector, whose quantum efficiency epsilon(gamma) for 662 keV gamma-rays is found to be 0.00175 and largely independent of detector bias, the quantum efficiency of the MCP detector is strongly dependent on the detector bias, with a power law index of 5.5. Background counts in MCP detectors from penetrating radiation can be reduced using MCP geometries with higher pitch and smaller channel diameter.
C1 [Funsten, Herbert O.] Los Alamos Natl Lab, Intelligence & Space Res Div, Los Alamos, NM 87545 USA.
[Harper, Ronnie W.; Larsen, Brian A.; Skoug, Ruth M.] Los Alamos Natl Lab, Intelligence & Space Res Div, Los Alamos, NM 87545 USA.
[Dors, Eric E.] Los Alamos Natl Lab, Emerging Threats Program Off, Los Alamos, NM 87545 USA.
[Janzen, Paul A.] Univ Montana, Dept Phys & Astron, Missoula, MT 59812 USA.
[MacDonald, Elizabeth A.] Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Poston, David I.] Los Alamos Natl Lab, Syst Design & Anal Grp, Los Alamos, NM 87545 USA.
[Ritzau, Stephen M.] Photonis USA Inc, Sturbridge, MA 01566 USA.
[Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Funsten, HO (reprint author), Los Alamos Natl Lab, Intelligence & Space Res Div, POB 1663, Los Alamos, NM 87545 USA.
EM hfun-sten@lanl.gov; rharper@lanl.gov; edors@lanl.gov;
paul.janzen@umontana.edu; balarsen@lanl.gov;
elizabeth.a.mac-donald@nasa.gov; poston@lanl.gov;
S.Ritzau@usa.photonis.com; rskoug@lanl.gov; thomasz@umich.edu
OI Funsten, Herbert/0000-0002-6817-1039
FU U.S. Department of Energy
FX Work at Los Alamos was enabled by the Laboratory Directed Research and
Development Program and performed under the auspices of the U.S.
Department of Energy.
NR 42
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U1 2
U2 10
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 OCT
PY 2015
VL 62
IS 5
BP 2283
EP 2293
DI 10.1109/TNS.2015.2464174
PN 2
PG 11
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA CU0XU
UT WOS:000363243200019
ER
PT J
AU Schioppa, EJ
Idarraga, J
van Beuzekom, M
Visser, J
Koffeman, E
Heijne, E
Engel, KJ
Uher, J
AF Schioppa, E. J.
Idarraga, J.
van Beuzekom, M.
Visser, J.
Koffeman, E.
Heijne, E.
Engel, K. J.
Uher, J.
TI Study of Charge Diffusion in a Silicon Detector Using an Energy
Sensitive Pixel Readout Chip
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE Charge sharing; diffusion; semiconductor detectors; timepix; x-ray
imaging
ID MEDIPIX2 DEVICE; PARTICLES
AB A 300 mu m thick thin p-on-n silicon sensor was connected to an energy sensitive pixel readout ASIC and exposed to a beam of highly energetic charged particles. By exploiting the spectral information and the fine segmentation of the detector, we were able to measure the evolution of the transverse profile of the charge carriers cloud in the sensor as a function of the drift distance from the point of generation. The result does not rely on model assumptions or electric field calculations. The data are also used to validate numerical simulations and to predict the detector spectral response to an X-ray fluorescence spectrum for applications in X-ray imaging.
C1 [Schioppa, E. J.; Idarraga, J.; van Beuzekom, M.; Visser, J.; Koffeman, E.] Nikhef, NL-1098 XG Amsterdam, Netherlands.
[Schioppa, E. J.] Univ Geneva, DPNC, Geneva, Switzerland.
[Idarraga, J.] NASA, New York, NY USA.
[Heijne, E.] Nikhef, European Ctr Nucl Res, Geneva, Switzerland.
[Heijne, E.] Czech Tech Univ, CERN, CR-16635 Prague, Czech Republic.
[Heijne, E.] Czech Tech Univ, IEAP, CR-16635 Prague, Czech Republic.
[Engel, K. J.] Philips Res Eindhoven, Amsterdam, Netherlands.
[Uher, J.] ASI, Amsterdam, Netherlands.
RP Schioppa, EJ (reprint author), Nikhef, Sci Pk 105, NL-1098 XG Amsterdam, Netherlands.
EM en-rico.junior.schioppa@cern.ch
OI Schioppa, Enrico Junior/0000-0002-1369-9944
FU Foundation for Fundamental Research on Matter (FOM); Dutch Technology
Foundation (STW); Ministry of Economic Affairs [OTP 11956]; Netherlands
Organization for Scientific Research (NWO)
FX This work is part of a research program funded by the Foundation for
Fundamental Research on Matter (FOM), which is part of the Netherlands
Organization for Scientific Research (NWO). The research has been
supported by the Dutch Technology Foundation (STW), which is the applied
science division of NWO, and the Technology Programme of the Ministry of
Economic Affairs, Project OTP 11956.
NR 22
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U1 3
U2 8
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD OCT
PY 2015
VL 62
IS 5
BP 2349
EP 2359
DI 10.1109/TNS.2015.2475124
PN 2
PG 11
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA CU0XU
UT WOS:000363243200027
ER
PT J
AU Krall, J
Menzies, T
Davies, M
AF Krall, Joseph
Menzies, Tim
Davies, Misty
TI GALE: Geometric Active Learning for Search-Based Software Engineering
SO IEEE TRANSACTIONS ON SOFTWARE ENGINEERING
LA English
DT Article
DE Multi-objective optimization; search based software engineering; active
learning
ID MULTIOBJECTIVE EVOLUTIONARY ALGORITHM; DIFFERENTIAL EVOLUTION;
OPTIMIZATION; SYSTEMS; MOEA/D
AB Multi-objective evolutionary algorithms (MOEAs) help software engineers find novel solutions to complex problems. When automatic tools explore too many options, they are slow to use and hard to comprehend. GALE is a near-linear time MOEA that builds a piecewise approximation to the surface of best solutions along the Pareto frontier. For each piece, GALE mutates solutions towards the better end. In numerous case studies, GALE finds comparable solutions to standard methods (NSGA-II, SPEA2) using far fewer evaluations (e.g. 20 evaluations, not 1,000). GALE is recommended when a model is expensive to evaluate, or when some audience needs to browse and understand how an MOEA has made its conclusions.
C1 LoadIQ, Reno, NV 89501 USA.
[Menzies, Tim] N Carolina State Univ, Comp Sci, Raleigh, NC 27695 USA.
[Davies, Misty] NASA, Ames Res Ctr, Intelligent Syst Div, Los Angeles, CA USA.
RP Krall, J (reprint author), LoadIQ, Reno, NV 89501 USA.
EM kralljoe@gmail.com; tim.menzies@gmail.com; misty.d.davies@nasa.gov
OI Davies, Misty/0000-0002-6245-9568
FU US National Science Foundation (NSF) [CCF:1017330]; Qatar/West Virginia
University research grant [NPRP 09-12-5-2-470]; NASA Ames Research
Center
FX The authors wish to thank the anonymous reviewers of this paper for
their many excellent suggestions on how to improve this paper. The work
was funded by the US National Science Foundation (NSF) grant CCF:1017330
and the Qatar/West Virginia University research grant NPRP
09-12-5-2-470. This research was partially conducted at NASA Ames
Research Center. Reference herein to any specific commercial product,
process, or service by trade name, trademark, manufacturer, or
otherwise, does not constitute or imply its endorsement by the United
States Government.
NR 63
TC 4
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U1 1
U2 4
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0098-5589
EI 1939-3520
J9 IEEE T SOFTWARE ENG
JI IEEE Trans. Softw. Eng.
PD OCT
PY 2015
VL 41
IS 10
BP 1001
EP 1018
DI 10.1109/TSE.2015.2432024
PG 18
WC Computer Science, Software Engineering; Engineering, Electrical &
Electronic
SC Computer Science; Engineering
GA CU0VR
UT WOS:000363237500004
ER
PT J
AU Wei, J
Wang, AA
Lambert, JL
Wettergreen, D
Cabrol, N
Warren-Rhodes, K
Zacny, K
AF Wei, Jie
Wang, Alian
Lambert, James L.
Wettergreen, David
Cabrol, Nathalie
Warren-Rhodes, Kimberley
Zacny, Kris
TI Autonomous soil analysis by the Mars Micro-beam Raman Spectrometer
(MMRS) on-board a rover in the Atacama Desert: a terrestrial test for
planetary exploration
SO JOURNAL OF RAMAN SPECTROSCOPY
LA English
DT Article; Proceedings Paper
CT 11th International GeoRaman Conference
CY JUN 15-19, 2014
CL St Louis, MI
DE Mars Micro-beam Raman Spectrometer; rover; soil; Atacama Desert
ID IDENTIFICATION; CARBONATE; GYPSUM; LIFE; TEMPERATURE; SPECTROSCOPY;
CASO4.2H2O; SEARCH; IMPACT; REGION
AB Laser Raman spectroscopy (LRS) has been proposed for in situ characterization of molecular species in planetary surface exploration, and three laser Raman spectrometers are included in the science payloads of two under-development missions to Mars (ESA-ExoMars2018 and NASA-Mars2020). We report the first rover test of a laser Raman spectrometer developed for flight, the Mars Micro-beam Raman Spectrometer (MMRS) in the Atacama Desert (Chile). The MMRS was integrated on the Zoe rover and analyzed subsurface samples brought up by a 1m drill and delivered by a carousel. The MMRS demonstrated robust performance over 50-km traverse on rugged terrains. From MMRS data, igneous minerals, carbonates, sulfates and carbonaceous materials were unambiguously identified. Quantified distributions of major minerals and carbonaceous materials are extracted from MMRS results, which can be used to imply the regional geological evolution, and potential bioactivities. MMRS in the field performed as well as an LRS laboratory instrument when MMRS was focused satisfactorily. The discovery of stable -anhydrite, in large quantity (20% in a sample), in the Atacama soils raises an important question of its stability in the field in a natural environment that is worth further laboratory experimental investigation. Copyright (c) 2015 John Wiley & Sons, Ltd.
C1 [Wei, Jie; Wang, Alian] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Wei, Jie; Wang, Alian] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
[Lambert, James L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wettergreen, David] Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA.
[Cabrol, Nathalie; Warren-Rhodes, Kimberley] NASA, SETI Inst, Carl Sagan Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Zacny, Kris] HoneyBee Robot & Spacecraft Mech Corp, Pasadena, CA 91103 USA.
RP Wei, J (reprint author), Washington Univ, Dept Earth & Planetary Sci, 1 Brookings Dr, St Louis, MO 63130 USA.
EM jiewei@levee.wustl.edu
FU NASA [NNX09AE80A, NNX13AM22G]; Department of Earth and Planetary
Sciences at Washington University in St. Louis; McDonnell Center for
Space Sciences at Washington University in St. Louis; Division 42 of Jet
Propulsion Laboratory; Division 38 of Jet Propulsion Laboratory
FX We gratefully acknowledge NASA support through ASTEP fund NNX09AE80A and
MATISSE fund NNX13AM22G. We thank the members of LITA Science team
(Gredon Foil, Edmond Grin, Trent Hare, Jeffrey Moersch, Kenneth Tanaka,
Christopher Tate and David Thompson), the members of LITA engineering
team (James Teza, David Kohanbash, Srinivasan Vijayarangan, Gale
Paulsen, Bolek Mellerowicz, Sean Yoon, Jack Craf and Magnus Hedlund) and
LiTA team's Chilean collaborators Dr. Guillermo Chong and Dr. Cecilia
Demergasso. We appreciate very much the generous supports that have been
given by the Department of Earth and Planetary Sciences and the
McDonnell Center for Space Sciences at Washington University in St.
Louis, and by the Division 42 and 38 of Jet Propulsion Laboratory to
MMRS-CIRS project.
NR 50
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U1 8
U2 30
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0377-0486
EI 1097-4555
J9 J RAMAN SPECTROSC
JI J. Raman Spectrosc.
PD OCT
PY 2015
VL 46
IS 10
SI SI
BP 810
EP 821
DI 10.1002/jrs.4656
PG 12
WC Spectroscopy
SC Spectroscopy
GA CT8TU
UT WOS:000363090200002
ER
PT J
AU Lee, SS
Wang, B
Waliser, DE
Neena, JM
Lee, JY
AF Lee, Sun-Seon
Wang, Bin
Waliser, Duane E.
Neena, Joseph Mani
Lee, June-Yi
TI Predictability and prediction skill of the boreal summer intraseasonal
oscillation in the Intraseasonal Variability Hindcast Experiment
SO CLIMATE DYNAMICS
LA English
DT Article
DE Boreal summer intraseasnal oscillation; Predictability; Prediction
skill; Intraseasonal Variability Hindcast Experiment (ISVHE)
ID MADDEN-JULIAN OSCILLATION; CLIMATE FORECAST SYSTEM; SEA-SURFACE
TEMPERATURE; WESTERN PACIFIC; COUPLED MODEL; SEASONAL-VARIATIONS; INDIAN
MONSOON; OCEAN; ATMOSPHERE; CONVECTION
AB Boreal summer intraseasonal oscillation (BSISO) is one of the dominant modes of intraseasonal variability of the tropical climate system, which has fundamental impacts on regional summer monsoons, tropical storms, and extra-tropical climate variations. Due to its distinctive characteristics, a specific metric for characterizing observed BSISO evolution and assessing numerical models' simulations has previously been proposed (Lee et al. in Clim Dyn 40:493-509, 2013). However, the current dynamical model's prediction skill and predictability have not been investigated in a multi-model framework. Using six coupled models in the Intraseasonal Variability Hindcast Experiment project, the predictability estimates and prediction skill of BSISO are examined. The BSISO predictability is estimated by the forecast lead day when mean forecast error becomes as large as the mean signal under the perfect model assumption. Applying the signal-to-error ratio method and using ensemble-mean approach, we found that the multi-model mean BSISO predictability estimate and prediction skill with strong initial amplitude (about 10 % higher than the mean initial amplitude) are about 45 and 22 days, respectively, which are comparable with the corresponding counterparts for Madden-Julian Oscillation during boreal winter (Neena et al. in J Clim 27:4531-4543, 2014a). The significantly lower BSISO prediction skill compared with its predictability indicates considerable room for improvement of the dynamical BSISO prediction. The estimated predictability limit is independent on its initial amplitude, but the models' prediction skills for strong initial amplitude is 6 days higher than the corresponding skill with the weak initial condition (about 15 % less than mean initial amplitude), suggesting the importance of using accurate initial conditions. The BSISO predictability and prediction skill are phase and season-dependent, but the degree of dependency varies with the models. It is important to note that the estimation of prediction skill depends on the methods that generate initial ensembles. Our analysis indicates that a better dispersion of ensemble members can considerably improve the ensemble mean prediction skills.
C1 [Lee, Sun-Seon; Wang, Bin] Univ Hawaii, Int Pacific Res Ctr, Dept Meteorol, Honolulu, HI 96822 USA.
[Wang, Bin] Nanjing Univ Informat Sci & Technol, Earth Syst Modeling Ctr NIAMS, Nanjing, Jiangsu, Peoples R China.
[Waliser, Duane E.; Neena, Joseph Mani] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Lee, June-Yi] Pusan Natl Univ, Inst Environm Studies, Busan, South Korea.
RP Wang, B (reprint author), Univ Hawaii, Int Pacific Res Ctr, Dept Meteorol, Honolulu, HI 96822 USA.
EM wangbin@hawaii.edu
FU NOAA/MAPP Project [NA10OAR4310247]; APEC climate center (APCC); National
Research Foundation (NRF) of Korea through a Global Research Laboratory
(GRL) grant of the Korean Ministry of Education, Science and Technology
(MEST) [2011-0021927]; Climate Dynamics Program of the National Science
Foundation [AGS-1005599]; NOAA/ESS program [NA13OAR4310167]; NOAA
Climate Program Office's CTB Program [GC10287a]; Office of Naval
Research [ONRBAA12-001]; NSF Climate and Large-Scale Dynamics Program
[AGS-1221013]; Indian Monsoon Mission
FX This work was jointly supported by the NOAA/MAPP Project Award Number
NA10OAR4310247, APEC climate center (APCC), and the National Research
Foundation (NRF) of Korea through a Global Research Laboratory (GRL)
grant of the Korean Ministry of Education, Science and Technology (MEST,
#2011-0021927). B.W. acknowledges support from Climate Dynamics Program
of the National Science Foundation under Award No. AGS-1005599 and
NOAA/ESS program, under Project NA13OAR4310167. Waliser and Neena were
supported by the NOAA Climate Program Office's CTB Program under grant
GC10287a, the Office of Naval Research under Project ONRBAA12-001, and
NSF Climate and Large-Scale Dynamics Program under Awards AGS-1221013
and the Indian Monsoon Mission. 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. This
is publication No. 9286 of the SOEST, publication No. 1105 of IPRC and
publication No. 038 of Earth System Modeling Center (ESMC).
NR 68
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U1 4
U2 6
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 OCT
PY 2015
VL 45
IS 7-8
BP 2123
EP 2135
DI 10.1007/s00382-014-2461-5
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CT2WV
UT WOS:000362667100026
ER
PT J
AU Bue, BD
Thompson, DR
Sellar, RG
Podest, EV
Eastwood, ML
Helmlinger, MC
McCubbin, IB
Morgan, JD
AF Bue, Brian D.
Thompson, David R.
Sellar, R. Glenn
Podest, Erika V.
Eastwood, Michael L.
Helmlinger, Mark C.
McCubbin, Ian B.
Morgan, John D.
TI Leveraging in-scene spectra for vegetation species discrimination with
MESMA-MDA
SO ISPRS JOURNAL OF PHOTOGRAMMETRY AND REMOTE SENSING
LA English
DT Article
DE Hyperspectral; Classification; Transformation; Modelling; Vegetation;
Agriculture
ID HYPERSPECTRAL IMAGE CLASSIFICATION; MIXTURE ANALYSIS MESMA;
FEATURE-EXTRACTION TECHNIQUES; NEAR-INFRARED-SPECTROSCOPY; ENDMEMBER
VARIABILITY; AVIRIS DATA; FOREST; CITRUS; SPECTROMETER; COVER
AB We describe an approach to improve Multiple Endmember Spectral Mixture Analysis (MESMA) results for applications involving discrimination among spectrally-similar species, and commonly occur in multispectral and hyperspectral vegetation remote sensing studies. Such applications are inherently difficult, due to the high degree of similarity between distinct species, coupled with potentially high intra-species variability caused by factors such as growing conditions, canopy structure, ambient illumination, or substrate characteristics. We describe a method to map spectra to a feature space where distinctions between plant species are emphasized using a transformation based on Multiclass Discriminant Analysis. We compute this transformation using groups of pixels that represent individual plant canopies similar to the endmembers in MESMA's spectral library, and describe a technique to automatically select such spectra from a given image. Compared to conventional MESMA, and also to several alternative MESMA formulations, we observe up to twofold increases in accuracy, along with a factor of ten reduction in computation time using our MESMA approach in several species discrimination applications. We demonstrate the effectiveness of our approach for agricultural species discrimination applications using spectra captured by two different imaging spectrometers. (C) 2015 International Society for Photogrammetry and Remote Sensing, Inc. (ISPRS). Published by Elsevier B.V. All rights reserved.
C1 [Bue, Brian D.; Thompson, David R.; Sellar, R. Glenn; Podest, Erika V.; Eastwood, Michael L.; Helmlinger, Mark C.; McCubbin, Ian B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morgan, John D.] Citrus Res Board, Riverside, CA 92057 USA.
RP Bue, BD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Brian.D.Bue@jpl.nasa.gov
FU California Citrus Research Board
FX This research was funded by the California Citrus Research Board and
conducted at the Jet Propulsion Laboratory, California Institute of
Technology. We thank Tracy L. Kahn and Peggy A. Mauk, both of the
University of California Riverside, for assistance in surveying the
Agricultural Experiment Station. The AVIRIS team, including Robert O.
Green and Sarah Lundeen of JPL, provided invaluable support for data
access and interpretation. We also thank the NGIS team for making it
possible to use their data. A portion of this research was carried out
at JPL by provision of a Space Act agreement under contract with the
National Aeronautics and Space Administration. Copyright 2014-2015. All
rights reserved.
NR 72
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U1 1
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0924-2716
EI 1872-8235
J9 ISPRS J PHOTOGRAMM
JI ISPRS-J. Photogramm. Remote Sens.
PD OCT
PY 2015
VL 108
BP 33
EP 48
DI 10.1016/j.isprsjprs.2015.06.001
PG 16
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
Photographic Technology
GA CT8OG
UT WOS:000363075300003
ER
PT J
AU Chen, S
Flatau, M
Jensen, TG
Shinoda, T
Schmidt, J
May, P
Cummings, J
Liu, M
Ciesielski, PE
Fairall, CW
Lien, RC
Baranowski, DB
Chi, NH
de Szoeke, S
Edson, J
AF Chen, Sue
Flatau, Maria
Jensen, Tommy G.
Shinoda, Toshiaki
Schmidt, Jerome
May, Paul
Cummings, James
Liu, Ming
Ciesielski, Paul E.
Fairall, Christopher W.
Lien, Ren-Chieh
Baranowski, Dariusz B.
Chi, Nan-Hsun
de Szoeke, Simon
Edson, James
TI A Study of CINDY/DYNAMO MJO Suppressed Phase
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Atmosphere-ocean interaction; Diurnal effects; Madden-Julian
oscillation; Oscillations; Coupled models; Model evaluation; performance
ID MADDEN-JULIAN OSCILLATION; COUPLED EQUATORIAL WAVES; TROPICAL WESTERN
PACIFIC; PREDICTION SYSTEM COAMPS; AIR-SEA INTERACTION; INTRASEASONAL
OSCILLATION; MOISTURE MODES; INDIAN-OCEAN; PROPAGATION; CONVECTION
AB The diurnal variability and the environmental conditions that support the moisture resurgence of MJO events observed during the Cooperative Indian Ocean Experiment on Intraseasonal Variability (CINDY)/DYNAMO campaign in October-December 2011 are investigated using in situ observations and the cloud-resolving fully air-ocean-wave Coupled Ocean-Atmosphere Mesoscale Prediction System (COAMPS). Spectral density and wavelet analysis of the total precipitable water (TPW) constructed from the DYNAMO soundings and TRMM satellite precipitation reveal a deep layer of vapor resurgence during the observed Wheeler and Hendon real-time multivariate MJO index phases 5-8 (MJO suppressed phase), which include diurnal, quasi-2-, quasi-3-4-, quasi-6-8-, and quasi-16-day oscillations. A similar oscillatory pattern is found in the DYNAMO moorings sea surface temperature analysis, suggesting a tightly coupled atmosphere and ocean system during these periods. COAMPS hindcast focused on the 12-16 November 2011 event suggests that both the diurnal sea surface temperature (SST) pumping and horizontal and vertical moisture transport associated with the westward propagating mixed Rossby-Gravity (MRG) waves play an essential role in the moisture resurgence during this period. Idealized COAMPS simulations of MRG waves are used to estimate the MRG and diurnal SST contributions to the overall moisture increase. These idealized MRG sensitivity experiments showed the TPW increase varies from 9% to 13% with the largest changes occurring in the simulations that included a diurnal SST variation of 2.5 degrees C as observed.
C1 [Chen, Sue; Flatau, Maria; Schmidt, Jerome; Liu, Ming] Naval Res Lab, Monterey, CA 93943 USA.
[Jensen, Tommy G.; Cummings, James] Stennis Space Ctr, Naval Res Lab, Hancock County, MS USA.
[Shinoda, Toshiaki] Texas A&M Univ, Corpus Christi, TX USA.
[May, Paul] Comp Sci Corp, Monterey, CA USA.
[Ciesielski, Paul E.] Colorado State Univ, Ft Collins, CO 80523 USA.
[Fairall, Christopher W.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Lien, Ren-Chieh; Chi, Nan-Hsun] Univ Washington, Seattle, WA 98195 USA.
[Baranowski, Dariusz B.] Univ Warsaw, Fac Phys, Inst Geophys, Warsaw, Poland.
[de Szoeke, Simon] Oregon State Univ, Corvallis, OR 97331 USA.
[Edson, James] Univ Connecticut, Groton, CT USA.
RP Chen, S (reprint author), Naval Res Lab, Marine Meteorol Div, 7 Grace Hopper Ave, Monterey, CA 93943 USA.
EM sue.chen@nrlmry.navy.mil
RI Shinoda, Toshiaki/J-3745-2016
OI Shinoda, Toshiaki/0000-0003-1416-2206
FU National Science Foundation; Office of Naval Research [601153N]; NOAA
CPO ESS program
FX We thank Scot Loehrer of National Center for Atmospheric Research (NCAR)
for assistance in acquiring the DYNAMO data. The sounding data was
provided by NCAR/EOL under sponsorship of the National Science
Foundation (http://data.eol.ucar.edu/). We appreciate Prof. James Moum
for providing the Revelle CTD data. Appreciation extends to Gilbert
Compo for helpful discussions on the use of wavelet analysis. Thanks go
to anonymous reviewers for helpful review of the manuscript. This
research is supported by the Office of Naval Research under Program
Element 601153N and partially supported by NOAA CPO ESS program. The
computing resource used for the real-time CINDY2011/DYNAMO COAMPS
forecast and subsequent COAMPS MJO studies are provided by the
Department of Defense High Performance Computing.
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U1 3
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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 OCT
PY 2015
VL 72
IS 10
BP 3755
EP 3779
DI 10.1175/JAS-D-13-0348.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CT2MY
UT WOS:000362637500002
ER
PT J
AU Oh, JH
Jiang, XN
Waliser, DE
Moncrieff, MW
Johnson, RH
Ciesielski, P
AF Oh, Ji-Hyun
Jiang, Xianan
Waliser, Duane E.
Moncrieff, Mitchell W.
Johnson, Richard H.
Ciesielski, Paul
TI A Momentum Budget Analysis of Westerly Wind Events Associated with the
Madden-Julian Oscillation during DYNAMO
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID PACIFIC WARM POOL; TOGA COARE IOP; ORGANIZED CONVECTIVE SYSTEMS; COUPLED
EQUATORIAL WAVES; MULTIVARIATE MJO INDEX; PART I; STRATIFORM
PRECIPITATION; INTRASEASONAL VARIATIONS; TROPICAL PACIFIC; KELVIN WAVES
AB The Dynamics of the Madden-Julian Oscillation (DYNAMO) field campaign was conducted over the Indian Ocean (IO) from October 2011 to February 2012 to investigate the initiation of the Madden-Julian oscillation (MJO). Three MJOs accompanying westerly wind events (WWEs) occurred in late October, late November, and late December 2011. Momentum budget analysis is conducted to understand the contributions of the dynamical processes involved in the wind evolution associated with the MJO over the IO during DYNAMO using European Centre for Medium-Range Weather Forecasts analysis. This analysis shows that westerly acceleration at lower levels associated with the MJO active phase generally appears to be maintained by the pressure gradient force (PGF), which could be partly canceled by meridional advection of the zonal wind. Westerly acceleration in the midtroposphere tends to be mostly attributable to vertical advection. The results herein imply that there is no simple linear dynamic model that can capture the WWEs associated with the MJO and that nonlinear processes have to be considered.In addition, the MJO in November (MJO2), accompanied by two WWEs (WWE1 and WWE2) spaced a few days apart, is diagnosed. Unlike other WWEs during DYNAMO, horizontal advection is more responsible for the westerly acceleration in the lower troposphere for WWE2 than the PGF. Interactions between the MJO2 envelope and convectively coupled waves (CCWs) are analyzed to illuminate the dynamical contribution of these synoptic-scale equatorial waves to the WWEs. The authors suggest that different developing processes among WWEs can be attributed to different types of CCWs.
C1 [Oh, Ji-Hyun; Jiang, Xianan; Waliser, Duane E.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Oh, Ji-Hyun; Jiang, Xianan; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Moncrieff, Mitchell W.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Johnson, Richard H.; Ciesielski, Paul] Colorado State Univ, Ft Collins, CO 80523 USA.
RP Oh, JH (reprint author), CALTECH, Jet Prop Lab, MS 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ji-hyun.oh@jpl.nasa.gov
FU NSF Climate and Large-Scale Dynamics Program [AGS-1228302, AGS-1221013,
AGS-1360237]; NOAA MAPP Program [NA12OAR4310075]; National Aeronautics
and Space Administration
FX We thank Drs. Chidong Zhang and Steve Williams for help with the ECWMF
DYNAMO operational analysis dataset. This work has greatly benefited
from stimulating discussions with Dr. D. Kim. We acknowledge support by
the NSF Climate and Large-Scale Dynamics Program under Awards
AGS-1228302, AGS-1221013, and AGS-1360237 and NOAA MAPP Program under
Award NA12OAR4310075. 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 72
TC 2
Z9 2
U1 0
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD OCT
PY 2015
VL 72
IS 10
BP 3780
EP 3799
DI 10.1175/JAS-D-15-0044.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CT2MY
UT WOS:000362637500003
ER
PT J
AU Kurowski, MJ
Grabowski, WW
Smolarkiewicz, PK
AF Kurowski, Marcin J.
Grabowski, Wojciech W.
Smolarkiewicz, Piotr K.
TI Anelastic and Compressible Simulation of Moist Dynamics at Planetary
Scales
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Anelastic models; Climate models; General circulation models; Model
comparison; Nonhydrostatic models
ID GENERAL-CIRCULATION; BAROCLINIC WAVES; DEEP CONVECTION; ENERGY-SPECTRA;
LIFE-CYCLES; EQUATIONS; MODEL; SOUNDPROOF; ATMOSPHERE; CORES
AB Moist anelastic and compressible numerical solutions to the planetary baroclinic instability and climate benchmarks are compared. The solutions are obtained by applying a consistent numerical framework for discrete integrations of the various nonhydrostatic flow equations. Moist extension of the baroclinic instability benchmark is formulated as an analog of the dry case. Flow patterns, surface vertical vorticity and pressure, total kinetic energy, power spectra, and total amount of condensed water are analyzed. The climate benchmark extends the baroclinic instability study by addressing long-term statistics of an idealized planetary equilibrium and associated meridional transports. Short-term deterministic anelastic and compressible solutions differ significantly. In particular, anelastic baroclinic eddies propagate faster and develop slower owing to, respectively, modified dispersion relation and abbreviated baroclinic vorticity production. These eddies also carry less kinetic energy, and the onset of their rapid growth occurs later than for the compressible solutions. The observed differences between the two solutions are sensitive to initial conditions as they diminish for large-amplitude excitations of the instability. In particular, on the climatic time scales, the anelastic and compressible solutions evince similar zonally averaged flow patterns with the matching meridional transports of entropy, momentum, and moisture.
C1 [Kurowski, Marcin J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grabowski, Wojciech W.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Smolarkiewicz, Piotr K.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
RP Kurowski, MJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 233-300, Pasadena, CA 91109 USA.
EM marcin.j.kurowski@jpl.nasa.gov
FU U.S. Department of Energy [DE-SC0006748]; National Aeronautics and Space
Administration; NSF Science and Technology Center for Multiscale
Modeling of Atmospheric Processes (CMMAP) [ATM-0425247]; European
Research Council under the European Union [320375]
FX Personal reviews from Drs. Christian Kuhnlein and Nils Wedi are
gratefully acknowledged. Comments from Prof. Rupert Klein and an
anonymous referee helped to improve the presentation. This material is
based upon work partially supported by the U.S. Department of Energy
under Award DE-SC0006748, and it was partially done during MJK's stay at
NCAR. Part of the research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. The views and
opinions of the authors expressed herein do not necessarily state or
reflect those of the U.S. government or any agency thereof. WWG was also
partially supported by the NSF Science and Technology Center for
Multiscale Modeling of Atmospheric Processes (CMMAP), managed by
Colorado State University under Cooperative Agreement ATM-0425247. PKS
acknowledges support by funding received from the European Research
Council under the European Union's Seventh Framework Programme
(FP7/2012/ERC Grant Agreement 320375).
NR 45
TC 5
Z9 5
U1 3
U2 9
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 OCT
PY 2015
VL 72
IS 10
BP 3975
EP 3995
DI 10.1175/JAS-D-15-0107.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CT2MY
UT WOS:000362637500014
ER
PT J
AU Suzuki, K
Stephens, G
Bodas-Salcedo, A
Wang, MH
Golaz, JC
Yokohata, T
Koshiro, T
AF Suzuki, Kentaroh
Stephens, Graeme
Bodas-Salcedo, Alejandro
Wang, Minghuai
Golaz, Jean-Christophe
Yokohata, Tokuta
Koshiro, Tsuyoshi
TI Evaluation of the Warm Rain Formation Process in Global Models with
Satellite Observations
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
DE Cloud microphysics; Climate models; Cloud parameterizations; Model
evaluation; performance; Single column models
ID CLIMATE MODEL; PART II; PARAMETERIZATION; CLOUDSAT; MICROPHYSICS;
SENSITIVITY; MULTISENSOR; SIMULATION; GROWTH; RADAR
AB This study examines the warm rain formation process over the global ocean in global climate models. Methodologies developed to analyze CloudSat and Moderate Resolution Imaging Spectroradiometer (MODIS) satellite observations are employed to investigate the cloud-to-precipitation process of warm clouds and are applied to the model results to examine how the models represent the process for warm stratiform clouds. Despite a limitation of the present study that compares the statistics for stratiform clouds in climate models with those from satellite observations, including both stratiform and (shallow) convective clouds, the statistics constructed with the methodologies are compared between the models and satellite observations to expose their similarities and differences. A problem common to some models is that they tend to produce rain at a faster rate than is observed. These model characteristics are further examined in the context of cloud microphysics parameterizations using a simplified one-dimensional model of warm rain formation that isolates key microphysical processes from full interactions with other processes in global climate models. The one-dimensional model equivalent statistics reproduce key characteristics of the global model statistics when corresponding autoconversion schemes are assumed in the one-dimensional model. The global model characteristics depicted by the statistics are then interpreted as reflecting behaviors of the autoconversion parameterizations adopted in the models. Comparisons of the one-dimensional model with satellite observations hint at improvements to the formulation of the parameterization scheme, thus offering a novel way of constraining key parameters in autoconversion schemes of global models.
C1 [Suzuki, Kentaroh] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778568, Japan.
[Stephens, Graeme] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bodas-Salcedo, Alejandro] Met Off Hadley Ctr, Exeter, Devon, England.
[Wang, Minghuai] Nanjing Univ, Inst Climate & Global Change Res, Nanjing 210008, Jiangsu, Peoples R China.
[Wang, Minghuai] Nanjing Univ, Sch Atmospher Sci, Nanjing 210008, Jiangsu, Peoples R China.
[Wang, Minghuai] Collaborat Innovat Ctr Climate Change, Nanjing, Jiangsu, Peoples R China.
[Golaz, Jean-Christophe] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Yokohata, Tokuta] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan.
[Koshiro, Tsuyoshi] Meteorol Res Inst, Tsukuba, Ibaraki 305, Japan.
RP Suzuki, K (reprint author), Univ Tokyo, Atmosphere & Ocean Res Inst, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778568, Japan.
EM ksuzuki@aori.u-tokyo.ac.jp
RI Suzuki, Kentaroh/C-3624-2011; Wang, Minghuai/E-5390-2011; Golaz,
Jean-Christophe/D-5007-2014; Koshiro, Tsuyoshi/O-7183-2016
OI Wang, Minghuai/0000-0002-9179-228X; Golaz,
Jean-Christophe/0000-0003-1616-5435; Koshiro,
Tsuyoshi/0000-0003-2971-7446
FU National Aeronautics and Space Administration (NASA) [NNN13D455T];
JAXA/EarthCARE project; Joint DECC/Defra Met Office Hadley Centre
Climate Programme [GA01101]; Department of Energy Office of Science,
Decadal and Regional Climate Prediction; DOE [DE-AC06-76RLO 1830];
Ministry of Education, Culture, Sports, Science and Technology of Japan
[23310014, 23340137]; Ministry of the Environment of Japan [S-10]
FX Part of this study was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration (NASA). Aspects of this study were
supported by NASA Grant NNN13D455T and JAXA/EarthCARE project. The
authors are grateful to three anonymous reviewers for their valuable
comments on earlier versions of this paper. K. Suzuki and A.
Bodas-Salcedo would like to thank Ian Boutle at the Met Office for his
guidance on microphysical process representation in HadGEM2. A.
Bodas-Salcedo was supported by the Joint DECC/Defra Met Office Hadley
Centre Climate Programme (GA01101). M. Wang was supported by the
Department of Energy Office of Science, Decadal and Regional Climate
Prediction using Earth System Models (EaSM) program and the Climate and
Earth System Modeling Program. The Pacific Northwest National Laboratory
(PNNL) is operated for the DOE by Battelle Memorial Institute under
contract DE-AC06-76RLO 1830. T. Yokohata was supported by the Program
for Risk Information on Climate Change, Grant-in-Aid 23310014 and
Grant-in-Aid 23340137 from the Ministry of Education, Culture, Sports,
Science and Technology of Japan, and by the Environment Research and
Technology Development Fund (S-10) of the Ministry of the Environment of
Japan. MIROC simulations were performed by Earth Simulator at JAMSTEC
and NEC SX at NIES.
NR 46
TC 2
Z9 2
U1 5
U2 21
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 OCT
PY 2015
VL 72
IS 10
BP 3996
EP 4014
DI 10.1175/JAS-D-14-0265.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CT2MY
UT WOS:000362637500015
ER
PT J
AU Cerracchio, P
Gherlone, M
Tessler, A
AF Cerracchio, Priscilla
Gherlone, Marco
Tessler, Alexander
TI Real-time displacement monitoring of a composite stiffened panel
subjected to mechanical and thermal loads
SO MECCANICA
LA English
DT Article
DE Shape sensing; Inverse Finite Element Method; Composite stiffened panel
ID FINITE-ELEMENT-METHOD; STRAIN; SHAPE; ALGORITHM; SENSORS; TECHNOLOGIES;
VELOCITY
AB Real-time reconstruction of the deformed structural shape using in situ strain measurements is an inverse problem, commonly called shape sensing. The knowledge of the deformed structural shape in real time has important implications for assessing strain, stress, and failure states, and thus constitutes a key component of structural health monitoring. In addition, shape sensing is required for control and actuation of smart structures. In this paper, shape sensing analyses are carried out for typical composite stiffened structures using the inverse Finite Element Method (iFEM). By using a limited set of discrete strain data, iFEM allows full-field reconstruction of displacements that can thus be monitored also far from sensor locations. First, the iFEM theoretical framework and the formulation of a triangular, inverse shell element are briefly discussed. Then, a general strain-sensor configuration amenable to stiffened shell structures is proposed. Several numerical results are presented for static, dynamic, and thermal loadings. The robustness of the method with respect to input errors is also investigated. It is shown that iFEM is a viable methodology for shape sensing of composite stiffened structures, having the desired computational efficiency, accuracy, and robustness with respect to strain-measurement errors. The iFEM shape-sensing methodology is particularly attractive because it does not require any information regarding applied loading, elastic material constants, inertial properties, or damping characteristics.
C1 [Cerracchio, Priscilla; Gherlone, Marco] Politecn Torino, Dept Mech & Aerosp Engn, I-10129 Turin, Italy.
[Tessler, Alexander] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
RP Cerracchio, P (reprint author), Politecn Torino, Dept Mech & Aerosp Engn, Corso Duca Abruzzi 24, I-10129 Turin, Italy.
EM priscilla.cerracchio@polito.it; marco.gherlone@polito.it;
Alexander.tessler-1@nasa.gov
OI Gherlone, Marco/0000-0002-5711-0046
NR 30
TC 1
Z9 1
U1 1
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0025-6455
EI 1572-9648
J9 MECCANICA
JI Meccanica
PD OCT
PY 2015
VL 50
IS 10
SI SI
BP 2487
EP 2496
DI 10.1007/s11012-015-0146-8
PG 10
WC Mechanics
SC Mechanics
GA CT7AS
UT WOS:000362966000003
ER
PT J
AU Tessler, A
AF Tessler, Alexander
TI Refined zigzag theory for homogeneous, laminated composite, and sandwich
beams derived from Reissner's mixed variational principle
SO MECCANICA
LA English
DT Article
DE Multi-scale theory; Refined zigzag theory; Reissner's mixed variational
principle; Composite beams; Sandwich beams; Compliant layer; Transverse
shear stress
ID CONTINUOUS INTERLAMINAR STRESSES; SHEAR-DEFORMATION-THEORY; PLATE
ELEMENT; DYNAMIC-RESPONSE; FINITE-ELEMENT; ORDER THEORY; DISPLACEMENT;
VIBRATION; SHELLS; MODEL
AB A highly accurate and computationally attractive shear-deformation theory for homogeneous, laminated composite, and sandwich laminates is developed for the linearly elastic analysis of planar beams. The theory is derived using the kinematic assumptions of Refined Zigzag Theory (RZT) and a two-step procedure that implements Reissner's Mixed Variational Theorem (RMVT). The basic expression for the transverse-shear stress that satisfies a priori the equlibrium conditions along the layer interfaces is obtained from Cauchy's equilibrium equations. The resulting transverse-shear stress consists of second-order derivatives of the two rotation variables of the theory, which subsequently are restated as the unknown stress functions. As the first step in fulfilling RMVT, the Lagrange-multiplier functional is minimized with respect to the unknown stress functions, resulting in the stress functions consisting of first-order derivatives of the kinematic variables. Subsequently, the second term of RMVT is minimized, producing four beam equilibrium equations and consistent boundary conditions. For any number of material layers the new theory maintains only four kinematic variables. The theory is labeled RZT((m)), where the superscript (m) stands for mixed formulation. The RZT((m)) can accurately model the axial stretch, bending, and transverse-shear deformations, without shear-correction factors. Analytic solutions are derived for simply supported beams subjected to transverse-normal and transverse-shear tractions on the top and bottom surfaces. It is demonstrated that RZT((m)) has a wide range of applicability which includes sandwich construction and the laminates with embedded thin compliant layers that can potentially model progression of delaminations. The main advantage of RZT((m)) over RZT is in the superior predictions of transverse-shear stresses that are obtained directly from the low-order transverse-shear strain measures of the theory without resorting to a post-processing integration procedure. Importantly, the methodology can be readily extended to plate theory, and it can be applied effectively for developing simple and efficient C-0-continuous finite elements.
C1 NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
RP Tessler, A (reprint author), NASA, Langley Res Ctr, Struct Mech & Concepts Branch, MS 190, Hampton, VA 23681 USA.
EM alexander.tessler-1@nasa.gov
FU Advanced Composites Project (ACP) at NASA Langley Research Center
FX The research reported herein was supported by the Advanced Composites
Project (ACP) at NASA Langley Research Center. The author would like to
thank his long-time collaborators, Professors Marco Di Sciuva and Marco
Gherlone, both of Politecnico di Torino, Italy, for the many fruitful
technical discussions related to this research. The author would also
like to thank his NASA colleague, Dr. Erik Saether, for his
computational support in obtaining exact elasticity solutions for the
problems examined in this paper.
NR 72
TC 3
Z9 3
U1 2
U2 9
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0025-6455
EI 1572-9648
J9 MECCANICA
JI Meccanica
PD OCT
PY 2015
VL 50
IS 10
SI SI
BP 2621
EP 2648
DI 10.1007/s11012-015-0222-0
PG 28
WC Mechanics
SC Mechanics
GA CT7AS
UT WOS:000362966000010
ER
PT J
AU Meyyappan, M
Koehne, JE
Han, JW
AF Meyyappan, M.
Koehne, Jessica E.
Han, Jin-Woo
TI Nanoelectronics and nanosensors for space exploration
SO MRS BULLETIN
LA English
DT Article
DE nanoscale; sensor; electronic material
ID WALLED CARBON NANOTUBES; FIELD-EMISSION TRIODE; LABEL-FREE DETECTION;
PHASE-CHANGE MEMORY; SENSOR ARRAY; CHEMICAL SENSORS; ELECTRONIC CHIP;
BIOSENSORS; NANOWIRE; GAS
AB Space missions have unique requirements for payloads of electronics, sensors, instruments, and other components in terms of mass, footprint, power consumption, and resistance to various types of radiation. Nanomaterials offer the potential for future radiation-hardened or radiation-immune electronics. Gas-sensing needs in planetary exploration and crew-cabin air-quality monitoring are currently being met by bulky instruments. Routine health checkups of astronauts and testing of water in space habitats are being done on a delayed basis by bringing samples back to Earth. Instead, nanomaterials can be used to construct ultrasmall, postage-stamp-sized gas/vapor sensors with selective discrimination and also lab-on-a-chip biosensors for water-quality monitoring and crew health monitoring.
C1 [Meyyappan, M.; Koehne, Jessica E.; Han, Jin-Woo] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
RP Meyyappan, M (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
EM m.meyyappan@nasa.gov; jessica.e.koehne@nasa.gov; jin-woo.han@nasa.gov
NR 69
TC 2
Z9 2
U1 4
U2 23
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0883-7694
EI 1938-1425
J9 MRS BULL
JI MRS Bull.
PD OCT
PY 2015
VL 40
IS 10
BP 822
EP 828
DI 10.1557/mrs.2015.223
PG 7
WC Materials Science, Multidisciplinary; Physics, Applied
SC Materials Science; Physics
GA CT6VS
UT WOS:000362951300011
ER
PT J
AU Siochi, EJ
Harrison, JS
AF Siochi, Emilie J.
Harrison, Joycelyn S.
TI Structural nanocomposites for aerospace applications
SO MRS BULLETIN
LA English
DT Article
DE Carbon; composite; nanostructure
ID ALIGNED CARBON NANOTUBES; REINFORCED POLYMER COMPOSITES;
SHEET/BISMALEIMIDE NANOCOMPOSITES; SHEET NANOCOMPOSITES; FIBER
COMPOSITES; IN-SITU; PERFORMANCE; DISPERSION; STRENGTH; POLYIMIDE
AB Carbon nanotubes (CNTs) have captured the imagination of the research community because of their many superior properties. In the nearly 25 years since their novelty was recognized, however, progress toward their utility as superlightweight structural materials, especially for aerospace applications, has been disappointing. Recent advancements have revived some of the anticipation for the touted systems payoffs. The purpose of this article is to examine how close CNTs have come to fulfilling expectations for lightweight aerospace structures in the two decades since the initial report stimulated intense interest in this material. This article also proposes areas of study to bridge knowledge gaps that can realize the potential for these CNT composites to be part of the lightweight structures technology suite for aerospace use.
C1 [Siochi, Emilie J.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
RP Siochi, EJ (reprint author), NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
EM emilie.j.siochi@nasa.gov; joycelyn.harrison@us.af.mil
NR 63
TC 4
Z9 4
U1 10
U2 29
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0883-7694
EI 1938-1425
J9 MRS BULL
JI MRS Bull.
PD OCT
PY 2015
VL 40
IS 10
BP 829
EP 835
DI 10.1557/mrs.2015.228
PG 7
WC Materials Science, Multidisciplinary; Physics, Applied
SC Materials Science; Physics
GA CT6VS
UT WOS:000362951300012
ER
PT J
AU Thibeault, SA
Kang, JH
Sauti, G
Park, C
Fay, CC
King, GC
AF Thibeault, Sheila A.
Kang, Jin Ho
Sauti, Godfrey
Park, Cheol
Fay, Catharine C.
King, Glen C.
TI Nanomaterials for radiation shielding
SO MRS BULLETIN
LA English
DT Article
DE composite; electron irradiation; nanostructure; neutron irradiation;
radiation effects
ID BORON-NITRIDE NANOTUBES; HYDROGEN STORAGE; CARBON NANOTUBES
AB This article reviews the application of nanomaterials for radiation shielding to protect humans from the hazards of radiation in space. The focus is on protection from space radiation, including galactic cosmic radiation (GCR), solar particle events (SPEs), and neutrons generated from the interactions of the GCR and SPEs with the intervening matter. Although the emphasis is on protecting humans, protection of electronics is also considered. There is a significant amount of work in the literature on materials for radiation shielding in terrestrial applications, such as for neutrons from nuclear reactors; however, the space environment poses additional and greater challenges because the incident particles can have high charges and extremely high energies. For materials to be considered for radiation shielding in space, they should perform more than just the radiation-shielding function; hence the emphasis is on multifunctional materials. In space, there is also the need for materials to be very lightweight and capable of surviving temperature extremes and withstanding mechanical loading. Nanomaterials could play a significant role as multifunctional radiation-shielding materials in space.
C1 [Thibeault, Sheila A.; Park, Cheol; King, Glen C.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
[Kang, Jin Ho; Sauti, Godfrey] Natl Inst Aerosp, Mountain View, CA USA.
[Fay, Catharine C.] NASA, Langley Res Ctr, Hampton, VA USA.
RP Thibeault, SA (reprint author), NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
EM sheila.a.thibeault@nasa.gov; jin.h.kang@nasa.gov;
godfrey.sauti-1@nasa.gov; cheol.park-1@nasa.gov;
catharine.c.fay@nasa.gov; glen.c.king@nasa.gov
NR 28
TC 7
Z9 7
U1 4
U2 42
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0883-7694
EI 1938-1425
J9 MRS BULL
JI MRS Bull.
PD OCT
PY 2015
VL 40
IS 10
BP 836
EP 841
DI 10.1557/mrs.2015.225
PG 6
WC Materials Science, Multidisciplinary; Physics, Applied
SC Materials Science; Physics
GA CT6VS
UT WOS:000362951300013
ER
PT J
AU Hayashi, M
Ly, C
Shimasaku, K
Motohara, K
Malkan, MA
Nagao, T
Kashikawa, N
Goto, R
Naito, Y
AF Hayashi, Masao
Ly, Chun
Shimasaku, Kazuhiro
Motohara, Kentaro
Malkan, Matthew A.
Nagao, Tohru
Kashikawa, Nobunari
Goto, Ryosuke
Naito, Yoshiaki
TI Physical conditions of the interstellar medium in star-forming galaxies
at z similar to 1.5
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: ISM; galaxies:
star formation
ID MASS-METALLICITY RELATION; NEAR-INFRARED SPECTROSCOPY; EMISSION-LINE
GALAXIES; DIGITAL SKY SURVEY; GRAVITATIONALLY LENSED GALAXIES; ALPHA
LUMINOSITY FUNCTION; ACTIVE GALACTIC NUCLEI; FRAME OPTICAL-SPECTRA; HIGH
IONIZATION STATE; LYMAN-BREAK GALAXIES
AB We present results from Subaru Fiber Multi Object Spectrograph near-infrared spectroscopy of 118 star-forming galaxies at z similar to 1.5 in the Subaru Deep Field. These galaxies are selected as [O II]lambda 3727 emitters at z approximate to 1.47 and 1.62 from narrow-band imaging. We detect the Ha emission line in 115 galaxies, the [O III]lambda 5007 emission line in 45 galaxies, and H beta, [N II]lambda 6584, and [S II]lambda lambda 6716, 6731 in 13, 16, and 6 galaxies, respectively. Including the [O II] emission line, we use the six strong nebular emission lines in the individual and composite rest-frame optical spectra to investigate the physical conditions of the interstellar medium in star-forming galaxies at z similar to 1.5. We find a tight correlation between Ha and [O II], which suggests that [O II] can be a good star formation rate indicator for galaxies at z similar to 1.5. The line ratios of H alpha/[O II] are consistent with those of local galaxies. We also find that [O II] emitters have strong [O III] emission lines. The [O III]/[O II] ratios are larger than normal star-forming galaxies in the local universe, suggesting a higher ionization parameter. Less massive galaxies have larger [O III]/[O II] ratios. With evidence that the electron density is consistent with local galaxies, the high ionization of galaxies athigh redshifts may be attributed to a harder radiation field by a young stellar population and/or an increase in the number of ionizing photons from each massive star.
C1 [Hayashi, Masao; Kashikawa, Nobunari] Natl Astron Observ, Opt & Infrared Astron Div, Mitaka, Tokyo 1818588, Japan.
[Ly, Chun] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Shimasaku, Kazuhiro; Goto, Ryosuke] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Shimasaku, Kazuhiro] Univ Tokyo, Res Ctr Early Univ, Bunkyo Ku, Tokyo 1130033, Japan.
[Motohara, Kentaro] Univ Tokyo, Grad Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan.
[Malkan, Matthew A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Nagao, Tohru] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan.
[Kashikawa, Nobunari] Grad Univ Adv Studies, Sch Sci, Dept Astron, Mitaka, Tokyo 1818588, Japan.
[Naito, Yoshiaki] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan.
RP Hayashi, M (reprint author), Natl Astron Observ, Opt & Infrared Astron Div, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
EM masao.hayashi@nao.ac.jp
FU Japan Society for the Promotion of Science (JSPS) through JSPS Research
Fellowship for Young Scientists; NASA
FX We thank Enrique Perez-Montero for reviewing our manuscript and
providing helpful comments, which improved the paper. The data used in
this paper were collected at the Subaru Telescope, which is operated by
the National Astronomical Observatory of Japan. We thank the Subaru
Telescope staff for their invaluable help in assisting our observations.
MH acknowledges support from the Japan Society for the Promotion of
Science (JSPS) through JSPS Research Fellowship for Young Scientists. CL
is funded through the NASA Postdoctoral Program.
NR 125
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U1 0
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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 OCT
PY 2015
VL 67
IS 5
AR 80
DI 10.1093/pasj/psv041
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CT5FL
UT WOS:000362834000002
ER
PT J
AU Momose, M
Morita, A
Fukagawa, M
Muto, T
Takeuchi, T
Hashimoto, J
Honda, M
Kudo, T
Okamoto, YK
Kanagawa, KD
Tanaka, H
Grady, CA
Sitko, ML
Akiyama, E
Currie, T
Follette, KB
Mayama, S
Kusakabe, N
Abe, L
Brandner, W
Brandt, TD
Carson, JC
Egner, S
Feldt, M
Goto, M
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, SS
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, GR
Kuzuhara, M
Kwon, J
Matsuo, T
McElwain, MW
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, YH
Takami, M
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Wisniewski, J
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Momose, Munetake
Morita, Ayaka
Fukagawa, Misato
Muto, Takayuki
Takeuchi, Taku
Hashimoto, Jun
Honda, Mitsuhiko
Kudo, Tomoyuki
Okamoto, Yoshiko K.
Kanagawa, Kazuhiro D.
Tanaka, Hidekazu
Grady, Carol A.
Sitko, Michael L.
Akiyama, Eiji
Currie, Thayne
Follette, Katherine B.
Mayama, Satoshi
Kusakabe, Nobuhiko
Abe, Lyu
Brandner, Wolfgang
Brandt, Timothy D.
Carson, Joseph C.
Egner, Sebastian
Feldt, Markus
Goto, Miwa
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko S.
Henning, Thomas
Hodapp, Klaus W.
Ishii, Miki
Iye, Masanori
Janson, Markus
Kandori, Ryo
Knapp, Gillian R.
Kuzuhara, Masayuki
Kwon, Jungmi
Matsuo, Taro
McElwain, Michael W.
Miyama, Shoken
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishimura, Tetsuo
Pyo, Tae-Soo
Serabyn, Eugene
Suenaga, Takuya
Suto, Hiroshi
Suzuki, Ryuji
Takahashi, Yasuhiro H.
Takami, Michihiro
Takato, Naruhisa
Terada, Hiroshi
Thalmann, Christian
Tomono, Daigo
Turner, Edwin L.
Watanabe, Makoto
Wisniewski, John
Yamada, Toru
Takami, Hideki
Usuda, Tomonori
Tamura, Motohide
TI Detailed structure of the outer disk around HD169142 with polarized
light in H-band
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE infrared: planetary systems; planet-disk interactions; protoplanetary
disks; stars: individual (HD 169142); stars: pre-main-sequence
ID 2-DIMENSIONAL RADIATIVE-TRANSFER; PLANET-FORMING REGIONS; MAIN-SEQUENCE
STARS; HERBIG AE/BE STARS; PROTOPLANETARY DISK; SCATTERED-LIGHT;
TRANSITIONAL DISK; PROTOSTELLAR ENVELOPES; CIRCUMSTELLAR DISKS; GIANT
PLANET
AB Coronagraphic imagery of the circumstellar disk around HD 169142 in H-band polarized intensity (PI) with Subaru/HiCIAO is presented. The emission scattered by dust particles at the disk surface in 0".2 <= r <= 1".2, or 29 <= r <= 174 AU, is successfully detected. The azimuthally-averaged radial profile of the PI shows a double power-law distribution, in which the PIs in r=29-52 AU and r=81.2-145 AU respectively show r(-3)-dependence. These two power-law regions are connected smoothly with a transition zone (TZ), exhibiting an apparent gap in r=40-70 AU. The PI in the inner power-law region shows a deep minimum whose location seems to coincide with the point source at lambda = 7 mm. This can be regarded as another sign of a protoplanet in TZ. The observed radial profile of the PI is reproduced by a minimally flaring disk with an irregular surface density distribution or with an irregular temperature distribution or with the combination of both. The depletion factor of surface density in the inner power-law region (r<50 AU) is derived to be >= 0.16 from a simple model calculation. The obtained PI image also shows small scale asymmetries in the outer power-law region. Possible origins for these asymmetries include corrugation of the scattering surface in the outer region, and shadowing effect by a puffed up structure in the inner power-law region.
C1 [Momose, Munetake; Morita, Ayaka; Okamoto, Yoshiko K.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Fukagawa, Misato] Osaka Univ, Grad Sch Sci, Toyonaka, Osaka 5600043, Japan.
[Muto, Takayuki] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan.
[Takeuchi, Taku; Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Hashimoto, Jun; Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Honda, Mitsuhiko] Kanagawa Univ, Dept Math & Phys, Hiratsuka, Kanagawa 2591293, Japan.
[Kudo, Tomoyuki; Currie, Thayne; Egner, Sebastian; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko S.; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo] Subaru Telescope, Hilo, HI 96720 USA.
[Kanagawa, Kazuhiro D.; Tanaka, Hidekazu] Hokkaido Univ, Inst Low Temp Sci, Sapporo, Hokkaido 0600819, Japan.
[Grady, Carol A.; McElwain, Michael W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Grady, Carol A.] Eureka Sci, Oakland, CA 96002 USA.
[Grady, Carol A.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Sitko, Michael L.] Space Sci Inst, Boulder, CO 80301 USA.
[Sitko, Michael L.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
[Akiyama, Eiji; Kusakabe, Nobuhiko; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Suenaga, Takuya; Suto, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro H.; Takami, Hideki; Usuda, Tomonori; Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Follette, Katherine B.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Mayama, Satoshi] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan.
[Mayama, Satoshi; Suenaga, Takuya] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
[Abe, Lyu] Univ Nice Sophia Antipolis, Lab Lagrange, CNRS, UMR 7293,Observ Cote Azur, F-06108 Nice 2, France.
[Brandner, Wolfgang; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Brandt, Timothy D.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA.
[Carson, Joseph C.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Goto, Miwa] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Janson, Markus] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden.
[Knapp, Gillian R.; Moro-Martin, Amaya; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kwon, Jungmi; Takahashi, Yasuhiro H.; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto, Kyoto 6068502, Japan.
[Miyama, Shoken] Hiroshima Univ, Hiroshima 7398511, Japan.
[Moro-Martin, Amaya] CSIC, INTA, CAB, Dept Astrophys, Madrid 28850, Spain.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Thalmann, Christian] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Momose, M (reprint author), Ibaraki Univ, Coll Sci, 2-1-1 Bunkyo, Mito, Ibaraki 3108512, Japan.
EM momose@mx.ibaraki.ac.jp
RI Tanaka, Hidekazu/E-1226-2012; MIYAMA, Shoken/A-3598-2015; Watanabe,
Makoto/E-3667-2016;
OI Tanaka, Hidekazu/0000-0001-9659-658X; Watanabe,
Makoto/0000-0002-3656-4081; Kanagawa, Kazuhiro/0000-0001-7235-2417;
Feldt, Markus/0000-0002-4188-5242
FU MEXT KAKENHI [23103004, 23103005]; U.S. National Science Foundation
[1009203]
FX We are grateful to the referee for valuable comments that improved our
manuscript. This work is supported by MEXT KAKENHI Nos. 23103004 and
23103005, and by the U.S. National Science Foundation under Award No.
1009203. This research has made use of the SIMBAD database, operated at
CDS, Strasbourg, France. Part of this research was carried out during
the workshop "Recent Development in Studies of Protoplanetary Disks with
ALMA", hosted by the Institute of Low Temperature Science, Hokkaido
University.
NR 67
TC 4
Z9 4
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 OCT
PY 2015
VL 67
IS 5
AR 83
DI 10.1093/pasj/psv051
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CT5FL
UT WOS:000362834000005
ER
PT J
AU Papike, JJ
Burger, PV
Bell, AS
Shearer, CK
Le, L
Jones, J
AF Papike, James J.
Burger, Paul V.
Bell, Aaron S.
Shearer, Charles K.
Le, Loan
Jones, John
TI Normal to inverse transition in martian spinet: Understanding the
interplay between chromium, vanadium, and iron valence state
partitioning through a crystal-chemical lens
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Spinel; crystal chemistry; partitioning; vanadium; chromium; Invited
Centennial article
ID COMPARATIVE PLANETARY MINERALOGY; OXYGEN FUGACITY; DIFFERENTIATION
HISTORY; ISOTOPIC SYSTEMATICS; OLIVINE; BASALTS; REDOX; MELT; METEORITE;
MANTLE
AB Spinel is a very important rock-forming mineral that is found in basalts from Earth, Mars, the Earth's Moon, and basaltic meteorites. Spinel can be used as a sensitive indicator of petrologic and geochemical processes that occur in its host rock. This paper highlights the role of increasing fo(2) (from IW-1 to FMQ+2) in converting a >90% normal spinel to an similar to 25% magnetite (inverse) spinel the trajectory of D-V(spincel/melt) as it relates to the ratio of V3+/V4+ in the melt, and the crystal chemical attributes of the spinel that control the intrinsic compatibility of both V3+ and V4+. This work examines the nuances of the V partitioning and provides a crystal chemical basis for understanding Fe3+, Cr, and V substitution into the octahedral sites of spinel. Understanding this interplay is critical for using spinels as both indicators of planetary parentage and reconstructing the redox history of magmatic systems on the terrestrial planets. Three potential examples for this use are provided. In addition, this work helps explain the ubiquitous miscibility gap between spinels with changing tilvospinel contents.
C1 [Papike, James J.; Burger, Paul V.; Bell, Aaron S.; Shearer, Charles K.] Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Le, Loan] NASA, Lyndon B Johnson Space Ctr, JSC Engn Technol & Sci JETS, Houston, TX 77058 USA.
[Jones, John] NASA, Lyndon B 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 [NNX13AH85G]; National Science Foundation, Earth Sciences
[EAR-1128799]; Department of Energy, Geosciences [DE-FG02-94ER14466];
U.S. Department of Energy, Office of Science, Office of Basic Energy
Sciences [DE-AC02-06CH11357]
FX Support for this research came from NASA Cosmochemistry grant NNX13AH85G
to C.K.S. Thanks also to Johnson Space Center. In addition, portions of
this work were performed at GeoSoilEnviroCARS (Sector 13), Advanced
Photon Source (APS), Argonne National Laboratory. GeoSoilEnviroCARS is
supported by the National Science Foundation, Earth Sciences
(EAR-1128799) and Department of Energy, Geosciences (DE-FG02-94ER14466).
Use of the Advanced Photon Source was supported by the U.S. Department
of Energy, Office of Science, Office of Basic Energy Sciences, under
Contract No. DE-AC02-06CH11357.
NR 46
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U1 7
U2 15
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 OCT
PY 2015
VL 100
IS 10
BP 2018
EP 2025
DI 10.2138/am-2015-5208
PG 8
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA CT3GG
UT WOS:000362694600002
ER
PT J
AU Ferguson, FT
Johnson, NM
Nuth, JA
AF Ferguson, Frank T.
Johnson, Natasha M.
Nuth, Joseph A., III
TI On the Use of Fourier Transform Infrared (FT-IR) Spectroscopy and
Synthetic Calibration Spectra to Quantify Gas Concentrations in a
Fischer-Tropsch Catalyst System
SO APPLIED SPECTROSCOPY
LA English
DT Article
DE Fourier transform infrared spectroscopy; FT-IR spectroscopy;
Apodization; HITRAN database; Fischer-Tropsch reaction; FTT;
Calibration; Quantitative analysis
ID HIGH-TEMPERATURES; CHEMISTRY; EMISSIONS; PLATINUM; DATABASE; VAPOR; CO
AB One possible origin of prebiotic organic material is that these compounds were formed via Fischer Tropsch-type (FTT) reactions of carbon monoxide and hydrogen on silicate and oxide grains in the warm, inner-solar nebula. To investigate this possibility, an experimental system has been built in which the catalytic efficiency of different grain-analog materials can be tested. During such runs, the gas phase above these grain analogs is sampled using Fourier transform infrared (FT-IR) spectroscopy. To provide quantitative estimates of the concentration of these gases, a technique in which high-resolution spectra of the gases are calculated using the High-Resolution Transmission Molecular Absorption (HITRAN) database is used. Next, these spectra are processed via a method that mimics the processes giving rise to the instrumental line shape of the FT-IR spectrometer, including apodization, self-apodization, and broadening due to the finite resolution. The result is a very close match between the measured and computed spectra. This technique was tested using four major gases found in the FTT reactions: carbon monoxide, methane, carbon dioxide, and water. For the ranges typical of the FTT reactions, the carbon monoxide results were found to be accurate to within 5% and the remaining gases accurate to within 10%. These spectra can then be used to generate synthetic calibration data, allowing the rapid computation of the gas concentrations in the FTT experiments.
C1 [Ferguson, Frank T.] Catholic Univ Amer, Dept Chem, Washington, DC 20064 USA.
[Johnson, Natasha M.; Nuth, Joseph A., III] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
RP Ferguson, FT (reprint author), Catholic Univ Amer, Dept Chem, Washington, DC 20064 USA.
EM frank.t.ferguson@nasa.gov
FU NASA
FX The authors gratefully acknowledge support for this work from NASA's
Exobiology Program.
NR 23
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PU SAGE PUBLICATIONS INC
PI THOUSAND OAKS
PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA
SN 0003-7028
EI 1943-3530
J9 APPL SPECTROSC
JI Appl. Spectrosc.
PD OCT
PY 2015
VL 69
IS 10
BP 1157
EP 1169
DI 10.1366/15-07950
PG 13
WC Instruments & Instrumentation; Spectroscopy
SC Instruments & Instrumentation; Spectroscopy
GA CT2FO
UT WOS:000362617600006
PM 26449809
ER
PT J
AU Fricker, GA
Wolf, JA
Saatchi, SS
Gillespie, TW
AF Fricker, Geoffrey A.
Wolf, Jeffrey A.
Saatchi, Sassan S.
Gillespie, Thomas W.
TI Predicting spatial variations of tree species richness in tropical
forests from high-resolution remote sensing
SO ECOLOGICAL APPLICATIONS
LA English
DT Article
DE alpha diversity; Barro Colorado Island, Panama; high-resolution
satellite imagery; lidar; multiple regression models; remote sensing;
spatial scale; tree species richness; tropical forests
ID RAIN-FORESTS; NEOTROPICAL FOREST; SATELLITE IMAGERY; ASSESSING
BIODIVERSITY; HABITAT ASSOCIATIONS; CANOPY STRUCTURE; CLIMATE-CHANGE;
DRY FORESTS; DIVERSITY; LIDAR
AB There is an increasing interest in identifying theories, empirical data sets, and remote-sensing metrics that can quantify tropical forest alpha diversity at a landscape scale. Quantifying patterns of tree species richness in the field is time consuming, especially in regions with over 100 tree species/ha. We examine species richness in a 50-ha plot in Barro Colorado Island in Panama and test if biophysical measurements of canopy reflectance from high-resolution satellite imagery and detailed vertical forest structure and topography from light detection and ranging (lidar) are associated with species richness across four tree size classes (>1, 1-10, >10, and >20 cm dbh) and three spatial scales (1, 0.25, and 0.04 ha). We use the 2010 tree inventory, including 204 757 individuals belonging to 301 species of freestanding woody plants or 166 +/- 1.5 species/ha (mean +/- SE), to compare with remote-sensing data. All remote-sensing metrics became less correlated with species richness as spatial resolution decreased from 1.0 ha to 0.04 ha and tree size increased from 1 cm to 20 cm dbh. When all stems with dbh >1 cm in 1-ha plots were compared to remote-sensing metrics, standard deviation in canopy reflectance explained 13% of the variance in species richness. The standard deviations of canopy height and the topographic wetness index (TWI) derived from lidar were the best metrics to explain the spatial variance in species richness (15% and 24%, respectively). Using multiple regression models, we made predictions of species richness across Barro Colorado Island (BCI) at the 1-ha spatial scale for different tree size classes. We predicted variation in tree species richness among all plants (adjusted and trees with dbh >10 cm (adjusted r(2) = 0.25). However, the best model results were for understory trees and shrubs (dbh 1-10 cm) (adjusted r(2) = 0.52) that comprise the majority of species richness in tropical forests. Our results indicate that high-resolution remote sensing can predict a large percentage of variance in species richness and potentially provide a framework to map and predict alpha diversity among trees in diverse tropical forests.
C1 [Fricker, Geoffrey A.; Gillespie, Thomas W.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA.
[Wolf, Jeffrey A.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Fricker, GA (reprint author), Univ Calif Los Angeles, Dept Geog, 1255 Bunche Hall,Box 951524, Los Angeles, CA 90095 USA.
EM africker@g.ucla.edu
FU Smithsonian Tropical Research Institute; National Science Foundation
[DEB-0939907]; NSF Dissertation Improvement Grant [BCS-1333701];
National Science Foundation Dimensions of Biodiversity grant [1050680]
FX We thank Stephen Hubbell, Joseph Wright, Jim Dalling, Elena Lobo,
Suzanna Loo de Lao, Bob Stallard, and Richard Condit for help in
providing both airborne lidar data and forest census plot data on BCI.
Fernando Espirito-Santo provided valuable input on the analysis and
methods. The lidar data collection was made possible with financial
support from Smithsonian Tropical Research Institute and National
Science Foundation (DEB-0939907) to Jim Dalling. Geoffrey A. Fricker was
financially supported by the NSF Dissertation Improvement Grant (Award
No: BCS-1333701). Technical GIS programming assistance was provided by
Evan Lyons and Jida Wang. This research was also supported by the
Dimensions of Biodiversity Distributed Graduate Seminar Series made
possible by a National Science Foundation Dimensions of Biodiversity
grant (1050680) to Sandy Andelman and Julia Parish.
NR 64
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U1 8
U2 36
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1051-0761
EI 1939-5582
J9 ECOL APPL
JI Ecol. Appl.
PD OCT
PY 2015
VL 25
IS 7
BP 1776
EP 1789
DI 10.1890/14-1593.1
PG 14
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA CT1BR
UT WOS:000362532600003
PM 26591445
ER
PT J
AU Coleman, GN
Garbaruk, A
Spalart, PR
AF Coleman, G. N.
Garbaruk, A.
Spalart, P. R.
TI Direct Numerical Simulation, Theories and Modelling of Wall Turbulence
with a Range of Pressure Gradients
SO FLOW TURBULENCE AND COMBUSTION
LA English
DT Article; Proceedings Paper
CT 10th International Symposium on Engineering Turbulence Modelling and
Measurements (ETMM)
CY SEP, 2014
CL Marbella, SPAIN
DE Wall-bounded turbulence; Pressure gradient effects; Turbulence
simulation
ID BOUNDARY-LAYER; REYNOLDS-NUMBER; EDDY-VISCOSITY; CHANNEL FLOW;
STATISTICS
AB A Direct Numerical Simulation (DNS) of Couette-Poiseuille flow is presented and analyzed in two ways. First, we test four semi-theoretical proposals for universal behaviour of respectively the velocity, the mixing length, the eddy viscosity, and the turbulence-kinetic-energy production rate. The question is which one may carry over from zero pressure gradient, for which they all agree, to finite pressure gradients, in which case they conflict. The DNS results, which are consistent between the favorable and the adverse pressure gradients, do not agree precisely with any of the theoretical proposals, but fall between those based on velocity (i.e., the log law) and on production. We do not know of a physical explanation for this trend, which has implications for theory, modelling, and wall functions. The residual effect of pressure gradients on the velocity profile, taken at y (+)=50, is examined in a wide range of simulations and experiments, which almost all turn out to follow a weak but definite trend to fall in adverse gradients. The second use of the data is to assess the accuracy of two turbulence models of the Reynolds-Averaged Navier-Stokes (RANS) type. These models are used in two modes. In the traditional mode, only the U velocity component is non-zero, and it depends only on the wall-normal coordinate y. In the newer mode, the V and W components are non-zero and the flow is allowed to depend on the lateral coordinate z with periodic conditions, but still not on x or t. For both pure Couette flow and the Couette-Poiseuille case considered here, this set-up allows some RANS models with nonlinear constitutive relations to generate streamwise vortices, which fill the channel. The presence of the rolls in the RANS generally improves the agreement with DNS and experiment, both qualitatively since the vortices are a known feature of such flows, and quantitatively, especially in terms of mixing in the core region of the channel. The vortices raise the skin-friction coefficient on the adverse-pressure-gradient side by as much as 30 %, depending on the chosen spacing between vortices.
C1 [Coleman, G. N.] NASA, Langley Res Ctr, Computat AeroSci, Hampton, VA 23681 USA.
[Garbaruk, A.] St Petersburg State Polytech Univ, St Petersburg 195251, Russia.
[Spalart, P. R.] Boeing Commercial Airplanes, Seattle, WA 98124 USA.
RP Coleman, GN (reprint author), NASA, Langley Res Ctr, Computat AeroSci, Hampton, VA 23681 USA.
EM g.n.coleman@nasa.gov; agarbaruk@cfd.spbstu.ru;
philippe.r.spalart@boeing.com
FU Revolutionary Computational Aerosciences project under NASA's
Fundamental Aerodynamics program; UK/EPSRC HECToR system, via the UK
Turbulence Consortium (EPSRC) [EP/G069581/1]
FX This project was sponsored by the Revolutionary Computational
Aerosciences project under NASA's Fundamental Aerodynamics program. The
computations were performed on the NASA Advanced Supercomputing (NAS)
Division and the UK/EPSRC HECToR system, via the UK Turbulence
Consortium (EPSRC Grant EP/G069581/1). We are grateful to Dr. Roderick
Johnstone for his many contributions to this study.
NR 26
TC 1
Z9 1
U1 3
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1386-6184
EI 1573-1987
J9 FLOW TURBUL COMBUST
JI Flow Turbul. Combust.
PD OCT
PY 2015
VL 95
IS 2-3
SI SI
BP 261
EP 276
DI 10.1007/s10494-015-9621-5
PG 16
WC Thermodynamics; Mechanics
SC Thermodynamics; Mechanics
GA CS8UN
UT WOS:000362364500005
ER
PT J
AU Sullivan, JT
McGee, TJ
DeYoung, R
Twigg, LW
Sumnicht, GK
Pliutau, D
Knepp, T
Carrion, W
AF Sullivan, John T.
McGee, Thomas J.
DeYoung, Russell
Twigg, Laurence W.
Sumnicht, Grant K.
Pliutau, Denis
Knepp, Travis
Carrion, William
TI Results from the NASA GSFC and LaRC Ozone Lidar Intercomparison: New
Mobile Tools for Atmospheric Research
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
DE Troposphere; Ozone; Instrumentation; sensors; Lidars; Lidar observations
ID DIFFERENTIAL ABSORPTION LIDAR; STRATOSPHERIC OZONE; PROFILES;
EFFICIENCY; SYSTEMS
AB During a 2-week period in May 2014, the National Aeronautics and Space Administration (NASA) Goddard Space Flight Center Tropospheric Ozone Differential Absorption Lidar (GSFC TROPOZ DIAL) was situated near the NASA Langley Research Center (LaRC) Mobile Ozone Lidar (LMOL) and made simultaneous measurements for a continuous 15-h observation period in which six separate ozonesondes were launched to provide reference ozone profiles. Although each of these campaign-ready lidars has very different transmitter and receiver components, they produced very similar ozone profiles, which were mostly within 10% of each other and the ozonesondes. The observed column averages as compared to the ozonesondes also agree well and are within 8% of each other. A robust uncertainty analysis was performed, and the results indicate that there is no statistically significant systematic bias between the TROPOZ and LMOL instruments. With the extended measurements and ozonesonde launches, this intercomparison has yielded an in-depth evaluation of the precision and accuracy of the two new lidars. This intercomparison is also the first (to the best of the authors' knowledge) reported measurement intercomparison of two ground-based tropospheric ozone lidar systems within the United States.
C1 [Sullivan, John T.] Univ Maryland Baltimore Cty, Dept Atmospher Phys, Baltimore, MD 21228 USA.
[Sullivan, John T.] Joint Ctr Earth Syst Technol, Baltimore, MD USA.
[McGee, Thomas J.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA.
[DeYoung, Russell] NASA, Sci Directorate, Langley Res Ctr, Greenbelt, MD 20771 USA.
[Twigg, Laurence W.; Sumnicht, Grant K.; Pliutau, Denis; Knepp, Travis] Sci Syst & Applicat Inc, Lanham, MD USA.
[Carrion, William] Coherent Applicat Inc, Hampton, VA USA.
RP Sullivan, JT (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Mail Code 614, Greenbelt, MD 20771 USA.
EM john.t.sullivan@nasa.gov
FU NASA Tropospheric Chemistry Program; Tropospheric Ozone Lidar Network
(TOLNet); Maryland Department of the Environment [U00P7201032];
NOAA-CREST CCNY Foundation CREST Grant [NA11SEC481004]
FX The authors gratefully acknowledge the support for this study provided
by Jack Kaye (NASA HQ), the NASA Tropospheric Chemistry Program, the
Tropospheric Ozone Lidar Network (TOLNet), the Maryland Department of
the Environment (Contract U00P7201032), and the NOAA-CREST CCNY
Foundation CREST Grant (Contract NA11SEC481004). Also, thanks to Raymond
M. Hoff for providing extended discussions of lidar techniques.
NR 24
TC 4
Z9 4
U1 1
U2 3
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 OCT
PY 2015
VL 32
IS 10
BP 1779
EP 1795
DI 10.1175/JTECH-D-14-00193.1
PG 17
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA CT0UX
UT WOS:000362514000005
ER
PT J
AU Islam, T
Srivastava, PK
Dai, Q
Gupta, M
Jaafar, WZW
AF Islam, Tanvir
Srivastava, Prashant K.
Dai, Qiang
Gupta, Manika
Jaafar, Wan Zurina Wan
TI Stratiform/convective rain delineation for TRMM microwave imager
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Stratiform/convective rain; Precipitation type classification; Passive
microwave (PMW) sensor; Satellite measurements; Precipitation radar
(PR); Brightness temperature; Machine learning algorithms
ID STRATIFORM PRECIPITATION; RADIOMETER OBSERVATIONS; BRIGHTNESS
TEMPERATURE; CLASSIFICATION METHODS; PROFILING ALGORITHM; WEATHER RADAR;
REFLECTIVITY; INFORMATION; PERFORMANCE; VALIDATION
AB This article investigates the potential for using machine learning algorithms to delineate stratiform/convective (S/C) rain regimes for passive microwave imager taking calibrated brightness temperatures as only spectral parameters. The algorithms have been implemented for the Tropical Rainfall Measuring Mission (TRMM) microwave imager (TMI), and calibrated as well as validated taking the Precipitation Radar (PR) S/C information as the target class variables. Two different algorithms are particularly explored for the delineation. The first one is metaheuristic adaptive boosting algorithm that includes the real, gentle, and modest versions of the AdaBoost. The second one is the classical linear discriminant analysis that includes the Fisher's and penalized versions of the linear discriminant analysis. Furthermore, prior to the development of the delineation algorithms, a feature selection analysis has been conducted for a total of 85 features, which contains the combinations of brightness temperatures from 10 GHz to 85 GHz and some derived indexes, such as scattering index, polarization corrected temperature, and polarization difference with the help of mutual information aided minimal redundancy maximal relevance criterion (mRMR). It has been found that the polarization corrected temperature at 85 GHz and the features derived from the "addition" operator associated with the 85 GHz channels have good statistical dependency to the S/C target class variables. Further, it has been shown how the mRMR feature selection technique helps to reduce the number of features without deteriorating the results when applying through the machine learning algorithms. The proposed scheme is able to delineate the S/C rain regimes with reasonable accuracy. Based on the statistical validation experience from the validation period, the Matthews correlation coefficients are in the range of similar to 0.60-0.70. Since, the proposed method does not rely on any a priori information, this makes it very suitable for other microwave sensors having similar channels to the TMI. The method could possibly benefit the constellation sensors in the Global Precipitation Measurement (GPM) mission era. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Islam, Tanvir] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Islam, Tanvir] NOAA NESDIS Ctr Satellite Applicat & Res, College Pk, MD USA.
[Islam, Tanvir] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Srivastava, Prashant K.; Gupta, Manika] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Dai, Qiang] Univ Bristol, Dept Civil Engn, Bristol, Avon, England.
[Gupta, Manika] Univ Space Res Assoc, Columbia, MD USA.
[Jaafar, Wan Zurina Wan] Univ Malaya, Dept Civil Engn, Kuala Lumpur, Malaysia.
RP Islam, T (reprint author), NASA Jet Prop Lab, Earth Sci Sect 329B, M-S 183-518 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM tanvir.islam@jpl.nasa.gov
OI Islam, Tanvir/0000-0003-2429-3074
FU National Aeronautics and Space Administration (NASA); Fundamental
Research Grant Scheme, University of Malaya [FRGS-FP039-2014B]
FX The research described in this publication was carried out, in part, at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration
(NASA). The TRMM data used in this effort were acquired as part of the
NASA's Earth-Sun System Division and archived and distributed by the
Goddard Earth Sciences (GES) Data and Information Services Center (DISC)
Distributed Active Archive Center (DAAC). Dr. Wan Zurina Wan Jaafar is
supported through Fundamental Research Grant Scheme (Project no:
FRGS-FP039-2014B), University of Malaya.
NR 42
TC 1
Z9 1
U1 1
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
EI 1879-1824
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD OCT
PY 2015
VL 133
BP 25
EP 35
DI 10.1016/j.jastp.2015.07.009
PG 11
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA CT2CZ
UT WOS:000362610900004
ER
PT J
AU Rouhi, N
Jung-Kubiak, C
White, V
Wilson, D
Anderson, J
Marrese-Reading, C
Forouhar, S
AF Rouhi, Nima
Jung-Kubiak, Cecile
White, Victor
Wilson, Daniel
Anderson, John
Marrese-Reading, Colleen
Forouhar, Siamak
TI Fabrication of 3-D Silicon Microneedles Using a Single-Step DRIE Process
SO JOURNAL OF MICROELECTROMECHANICAL SYSTEMS
LA English
DT Article
DE 3D etch; silicon micro-structure; deep reactive ion etching; dual-angle;
gray-scale e-beam lithography
ID ELECTRON-BEAM LITHOGRAPHY; 3D; ARRAYS; MICROBATTERIES; DELIVERY; MICRO;
MEMS
AB Fabrication of 3-D microstructures is one of the most challenging aspects of silicon micromachining. In this paper, we present a novel microfabrication method using one single-step deep reactive ion etching process with gray-scale e-beam lithography mask that offers deeply etched (>350-mu m deep) dual-angle 3-D microneedles with control over the height and shape of the structures. Moreover, we found that the shape of the e-beam lithography patterns can determine the general configuration and features of the final etched microneedles, and that the etching process parameters have the most impact on the microneedles' shape, such as size and vertical base angle. Large arrays of 20 x 20 microneedles with height uniformity of better than 3% are fabricated. [2014-0209]
C1 [Rouhi, Nima; Jung-Kubiak, Cecile; White, Victor; Wilson, Daniel; Anderson, John; Marrese-Reading, Colleen; Forouhar, Siamak] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Rouhi, Nima] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
RP Rouhi, N (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM nrouhi@caltech.edu; cecile.d.jung@jpl.nasa.gov; vewhite@jpl.nasa.gov;
daniel.w.wilson@jpl.nasa.gov; John.R.Anderson@jpl.nasa.gov;
colleen.m.marrese-reading@jpl.nasa.gov; siamak.forouhar@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology, Pasadena,
CA, USA; National Aeronautics and Space Administration [105571]; U.S.
Government Sponsorship
FX This work was supported in part by the Jet Propulsion Laboratory,
California Institute of Technology, Pasadena, CA, USA, under a contract
with the National Aeronautics and Space Administration under Grant
105571, and in part by the U.S. Government Sponsorship. Subject Editor
R. Maboudian.
NR 29
TC 0
Z9 0
U1 5
U2 21
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1057-7157
EI 1941-0158
J9 J MICROELECTROMECH S
JI J. Microelectromech. Syst.
PD OCT
PY 2015
VL 24
IS 5
BP 1409
EP 1414
DI 10.1109/JMEMS.2015.2406878
PG 6
WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology;
Instruments & Instrumentation; Physics, Applied
SC Engineering; Science & Technology - Other Topics; Instruments &
Instrumentation; Physics
GA CS8RB
UT WOS:000362354900020
ER
PT J
AU Wedemeyer-Strombel, KR
Balazs, GH
Johnson, JB
Peterson, TD
Wicksten, MK
Plotkin, PT
AF Wedemeyer-Strombel, Kathryn R.
Balazs, George H.
Johnson, James B.
Peterson, Taylor D.
Wicksten, Mary K.
Plotkin, Pamela T.
TI High frequency of occurrence of anthropogenic debris ingestion by sea
turtles in the North Pacific Ocean
SO MARINE BIOLOGY
LA English
DT Article
ID NORTHWESTERN HAWAIIAN-ISLANDS; EASTERN TROPICAL PACIFIC; ZONE
CHLOROPHYLL FRONT; MARINE DEBRIS; CARETTA-CARETTA; PLASTIC DEBRIS;
FEEDING ECOLOGY; CHELONIA-MYDAS; LEPIDOCHELYS-OLIVACEA; PELAGIC HABITAT
AB Ingestion of anthropogenic debris can have deleterious effects on sea turtles. To study diet content of sea turtles, four species were opportunistically collected as deceased bycatch over 18 years (1993-2011) from pelagic longline fisheries based in American Samoa and Hawaii (North Pacific between 140A degrees-170A degrees W and 20A degrees S-50A degrees N). Diet contents were analyzed from 71 sea turtles: 45 olive ridleys (Lepidochelys olivacea), 22 greens (Chelonia mydas), 2 loggerheads (Caretta caretta), and 2 leatherbacks (Dermochelys coriacea). This study reports some of the highest frequencies of anthropogenic debris ingestion documented for sea turtles, with 83 % of all the sea turtles sampled ingesting anthropogenic debris. Within species, 91 % of greens and 82 % of olive ridleys ingested anthropogenic debris. This is the first published report of anthropogenic debris ingestion by olive ridleys outside of the Atlantic Ocean. Neither of the leatherbacks ingested anthropogenic debris. The average dry weight of anthropogenic debris ingested by individual olive ridleys and individual greens was 4 and 7 g, respectively. The total dry weights of anthropogenic debris ingested by the two loggerheads were 9 and 120 g. Plastics were the most prominent anthropogenic debris ingested, making up 95 % (405 g dry weight) of the total 427 g ingested. Increased ingestion of anthropogenic debris was found in olive ridleys collected during the winter, which corresponds with the wintertime increase in anthropogenic debris accumulated in the North Pacific Subtropical Convergence Zone. This study highlights the need to better understand the factors affecting anthropogenic debris ingestion and its sublethal effects.
C1 [Wedemeyer-Strombel, Kathryn R.] Texas A&M Univ, Dept Wildlife & Fisheries Sci, College Stn, TX 77842 USA.
[Balazs, George H.] Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96818 USA.
[Johnson, James B.] Univ Oklahoma, Dept Biol, Norman, OK 73019 USA.
[Peterson, Taylor D.; Plotkin, Pamela T.] Texas A&M Univ, Dept Oceanog & Marine Biol, Grad Interdisciplinary Program, College Stn, TX 77843 USA.
[Wicksten, Mary K.] Texas A&M Univ, Dept Biol, College Stn, TX 77842 USA.
RP Wedemeyer-Strombel, KR (reprint author), Texas A&M Univ, Dept Wildlife & Fisheries Sci, 214C Heep Lab Bldg,TAMU 2258, College Stn, TX 77842 USA.
EM krwedemeyer@gmail.com
FU Texas A&M University Marine Biology Graduate Interdisciplinary Program;
Texas A&M University Department of Biology; National Science Foundation
[DGE-1252521]
FX We thank the Texas A&M University Marine Biology Graduate
Interdisciplinary Program and the Texas A&M University Department of
Biology for financial support for this research. This material is based
upon work supported by the National Science Foundation Graduate Research
Fellowship under Grant No. DGE-1252521. Any opinion, findings, and
conclusions or recommendations expressed in this material are those of
the authors and do not necessarily reflect the views of the National
Science Foundation. Special thanks to Jeffrey Seminoff, Tarla Rai
Peterson, Sarah Flanagan, Laura Edelstein, and Rachael Fajardo for
guidance during the writing process, and Brittany Schwartzkopf,
Charlayna Cammarata, and Samantha Trent for helpful comments on early
versions of the manuscript. Thomas DeWitt and Gil Rosenthal provided
usage of a drying oven, and Joseph Bernardo allowed access to dissection
equipment. Thank you to Bryan Wallace, Barbara Santer, and our three
reviewers, M. Frick, J. Senko and J. Tomas, for constructive comments on
this manuscript, especially in reference to reexamining seasonality.
NR 77
TC 3
Z9 4
U1 15
U2 67
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 0025-3162
EI 1432-1793
J9 MAR BIOL
JI Mar. Biol.
PD OCT
PY 2015
VL 162
IS 10
BP 2079
EP 2091
DI 10.1007/s00227-015-2738-1
PG 13
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA CS8FS
UT WOS:000362322200013
ER
PT J
AU Aponte, JC
Dworkin, JP
Elsila, JE
AF Aponte, Jose C.
Dworkin, Jason P.
Elsila, Jamie E.
TI Indigenous aliphatic amines in the aqueously altered Orgueil meteorite
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID CIRCULARLY-POLARIZED LIGHT; CARBON-ISOTOPE COMPOSITION; SPARK DISCHARGE
EXPERIMENT; COMPOUND-SPECIFIC CARBON; MURCHISON METEORITE; ENANTIOMERIC
EXCESSES; MONOCARBOXYLIC ACIDS; PARENT BODY; ASYMMETRIC AUTOCATALYSIS;
ICE ANALOGS
AB The CI1 Orgueil meteorite is a highly aqueously altered carbonaceous chondrite. It has been extensively studied, and despite its extensive degree of aqueous alteration and some documented instances of contamination, several indigenous organic compounds including amino acids, carboxylic acids, and nucleobases have been detected in its carbon-rich matrix. We recently developed a novel gas chromatographic method for the enantiomeric and compound-specific isotopic analyses of meteoritic aliphatic monoamines in extracts and have now applied this method to investigate the monoamine content in Orgueil. We detected 12 amines in Orgueil, with concentrations ranging from 1.1 to 332 nmol g(-1) of meteorite and compared this amine content in Orgueil with that of the CM2 Murchison meteorite, which experienced less parent-body aqueous alteration. Methylamine is four times more abundant in Orgueil than in Murchison. As with other species, the amine content in Orgueil extracts shows less structural diversity than that in Murchison extracts. We measured the compound-specific stable carbon isotopic ratios (delta C-13) for 5 of the 12 monoamines detected in Orgueil and found a range of delta C-13 values from -20 to +59 parts per thousand. These delta C-13 values fall into the range of other meteoritic organic compounds, although they are C-13-depleted relative to their counterparts extracted from the Murchison meteorite. In addition, we measured the enantiomeric composition for the chiral monoamines (R)- and (S)-sec-butylamine in Orgueil, and found it was racemic within experimental error, in contrast with the L-enantiomeric excess found for its amino acid structural analog isovaline. The racemic nature of sec-butylamine in Orgueil was comparable to that previously observed in Murchison, and to other CM2 and CR2 carbonaceous chondrites measured in this work (ALH 83100 [CM1/2], LON 94101 [CM2], LEW 90500 [CM2], LAP 02342 [CR2], and GRA 95229 [CR2]). These results allow us to place some constraints on the effects of aqueous alteration observed over the monoamine concentrations in Orgueil and Murchison, and to evaluate the primordial synthetic relationships between meteoritic monoamines and amino acids.
C1 [Aponte, Jose C.; Dworkin, Jason P.; Elsila, Jamie E.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Aponte, Jose C.] Catholic Univ Amer, Dept Chem, Washington, DC 20064 USA.
RP Aponte, JC (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Code 691, Greenbelt, MD 20771 USA.
EM jose.c.aponte@nasa.gov
RI Elsila, Jamie/C-9952-2012; Dworkin, Jason/C-9417-2012
OI Dworkin, Jason/0000-0002-3961-8997
FU NSF; NASA; NASA Postdoctoral Program at the Goddard Space Flight Center;
NASA Astrobiology Institute through NASA; NASA Astrobiology Institute;
Goddard Center for Astrobiology, NASA's Cosmochemistry Program; Simons
Foundation (SCOL award) [302497]
FX U.S. 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. The authors thank P. Ehrenfreund for providing the
Orgueil meteorite sample used in this study, D. P. Glavin for his
helpful discussions, and Queenie H. S. Chan and an anonymous reviewer
for their insightful criticism and suggestions to improve the
manuscript. J. C. A. acknowledges the support from the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities and the NASA Astrobiology Institute through a
contract with NASA. This research was supported by the NASA Astrobiology
Institute and the Goddard Center for Astrobiology, NASA's Cosmochemistry
Program, and a grant from the Simons Foundation (SCOL award 302497 to J.
P. D.).
NR 90
TC 4
Z9 4
U1 2
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 OCT
PY 2015
VL 50
IS 10
BP 1733
EP 1749
DI 10.1111/maps.12507
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CT1JN
UT WOS:000362554700006
ER
PT J
AU Righter, K
Abell, P
Agresti, D
Berger, EL
Burton, AS
Delaney, JS
Fries, MD
Gibson, EK
Haba, MK
Harrington, R
Herzog, GF
Keller, LP
Locke, D
Lindsay, FN
Mccoy, TJ
Morris, RV
Nagao, K
Nakamura-Messenger, K
Niles, PB
Nyquist, LE
Park, J
Peng, ZX
Shih, CY
Simon, JI
Swisher, CC
Tappa, MJ
Turrin, BD
Zeigler, RA
AF Righter, K.
Abell, P.
Agresti, D.
Berger, E. L.
Burton, A. S.
Delaney, J. S.
Fries, M. D.
Gibson, E. K.
Haba, M. K.
Harrington, R.
Herzog, G. F.
Keller, L. P.
Locke, D.
Lindsay, F. N.
McCoy, T. J.
Morris, R. V.
Nagao, K.
Nakamura-Messenger, K.
Niles, P. B.
Nyquist, L. E.
Park, J.
Peng, Z. X.
Shih, C. -Y.
Simon, J. I.
Swisher, C. C., III
Tappa, M. J.
Turrin, B. D.
Zeigler, R. A.
TI Mineralogy, petrology, chronology, and exposure history of the
Chelyabinsk meteorite and parent body
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID HIGH-VELOCITY RESOLUTION; IMPACT-MELT BRECCIA; RUTHENIUM TETROXIDE
OXIDATION; ITOKAWA DUST PARTICLES; NEAR-EARTH ASTEROIDS; EARLY
SOLAR-SYSTEM; ORDINARY CHONDRITES; MOSSBAUER-SPECTROSCOPY; LL5
METEORITE; COMPOSITIONAL CLASSIFICATION
AB Three masses of the Chelyabinsk meteorite have been studied with a wide range of analytical techniques to understand the mineralogical variation and thermal history of the Chelyabinsk parent body. The samples exhibit little to no postentry oxidation via M_ ossbauer and Raman spectroscopy indicating their fresh character, but despite the rapid collection and care of handling some low levels of terrestrial contamination did nonetheless result. Detailed studies show three distinct lithologies, indicative of a genomict breccia. A light-colored lithology is LL5 material that has experienced thermal metamorphism and subsequent shock at levels near S4. The second lithology is a shock-darkened LL5 material in which the darkening is caused by melt and metal-troilite veins along grain boundaries. The third lithology is an impact melt breccia that formed at high temperatures (similar to 1600 degrees C), and it experienced rapid cooling and degassing of S2 gas. Portions of light and dark lithologies from Chel-101, and the impact melt breccias (Chel-102 and Chel-103) were prepared and analyzed for Rb-Sr, Sm-Nd, and Ar-Ar dating. When combined with results from other studies and chronometers, at least eight impact events (e.g., similar to 4.53 Ga, similar to 4.45 Ga, similar to 3.73 Ga, similar to 2.81 Ga, similar to 1.46 Ga, similar to 852 Ma, similar to 312 Ma, and similar to 27 Ma) are clearly identified for Chelyabinsk, indicating a complex history of impacts and heating events. Finally, noble gases yield young cosmic ray exposure ages, near 1 Ma. These young ages, together with the absence of measurable cosmogenic derived Sm and Cr, indicate that Chelyabinsk may have been derived from a recent breakup event on an NEO of LL chondrite composition.
C1 [Righter, K.; Abell, P.; Burton, A. S.; Fries, M. D.; Gibson, E. K.; Keller, L. P.; Morris, R. V.; Nakamura-Messenger, K.; Niles, P. B.; Nyquist, L. E.; Simon, J. I.; Zeigler, R. A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Agresti, D.] Univ Alabama Birmingham, Dept Phys, Birmingham, AL 35294 USA.
[Berger, E. L.] NASA, Lyndon B Johnson Space Ctr, GeoControl Syst Inc, Jacobs JETS Contract, Houston, TX 77058 USA.
[Delaney, J. S.; Herzog, G. F.; Lindsay, F. N.; Park, J.] Rutgers State Univ, Dept Chem & Chem Biol, Piscataway, NJ 08854 USA.
[Harrington, R.] NASA, Lyndon B Johnson Space Ctr, UTAS, Jacobs JETS Contract, Houston, TX 77058 USA.
[Locke, D.] NASA, Lyndon B Johnson Space Ctr, HX5, Jacobs JETS Contract, Houston, TX 77058 USA.
[McCoy, T. J.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Haba, M. K.; Nagao, K.] Univ Tokyo, Geochem Res Ctr, Bunkyo Ku, Tokyo 1130033, Japan.
[Peng, Z. X.] NASA, Lyndon B Johnson Space Ctr, Barrios Tech, Jacobs JETS Contract, Houston, TX 77058 USA.
[Shih, C. -Y.] NASA, Lyndon B Johnson Space Ctr, Jacobs JETS Contract, Houston, TX 77058 USA.
[Swisher, C. C., III; Turrin, B. D.] Rutgers State Univ, Dept Earth & Planetary Sci, Piscataway, NJ 08854 USA.
[Tappa, M. J.] NASA, Lyndon B Johnson Space Ctr, Aerodyne Ind, Jacobs JETS Contract, Houston, TX 77058 USA.
RP Righter, K (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
FU RTOP; Cosmochemistry program [11-COS11-0066]; NASA Lunar Advanced
Science Exploration Research (LASER) Program [10-LASER10-0054]
FX We thank T. Kryachko for donating Chel-101 and -102 to NASA, L. Johnson
and R. Landis for facilitating delivery of samples from Russia to
Houston, and M. Farmer for the Chel-103 sample. Rhian Jones kindly
shared Chelyabinsk samples (UNM 001h and 020) with us for the Ar dating.
This research was supported by an RTOP to K. Righter and 11-COS11-0066
to J.I. Simon from the Cosmochemistry program, financial support for
L.E. Nyquist and C.-Y. Shih was provided by the NASA Lunar Advanced
Science Exploration Research (LASER) Program via proposal number
10-LASER10-0054. Journal reviews of K. Welten and L. Folco helped
improve the presentation of this work.
NR 108
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U1 2
U2 12
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 OCT
PY 2015
VL 50
IS 10
BP 1790
EP 1819
DI 10.1111/maps.12511
PG 30
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CT1JN
UT WOS:000362554700009
ER
PT J
AU Holdaway, D
Errico, R
Gelaro, R
Kim, JG
Mahajan, R
AF Holdaway, Daniel
Errico, Ronald
Gelaro, Ronald
Kim, Jong G.
Mahajan, Rahul
TI A Linearized Prognostic Cloud Scheme in NASA's Goddard Earth Observing
System Data Assimilation Tools
SO MONTHLY WEATHER REVIEW
LA English
DT Article
DE Filtering techniques; Singular vectors; Variational analysis; Cloud
parameterizations; Convective parameterization; Data assimilation
ID 4-DIMENSIONAL VARIATIONAL ASSIMILATION; RELAXED ARAKAWA-SCHUBERT; MOIST
PHYSICS SCHEMES; CONVECTION SCHEME; MESOSCALE MODEL; INITIAL TESTS;
IMPACT; SCALE; 4D-VAR
AB A linearized prognostic cloud scheme has been developed to accompany the linearized convection scheme recently implemented in NASA's Goddard Earth Observing System data assimilation tools. The linearization, developed from the nonlinear cloud scheme, treats cloud variables prognostically so they are subject to linearized advection, diffusion, generation, and evaporation. Four linearized cloud variables are modeled, the ice and water phases of clouds generated by large-scale condensation and, separately, by detraining convection. For each species the scheme models their sources, sublimation, evaporation, and autoconversion. Large-scale, anvil and convective species of precipitation are modeled and evaporated. The cloud scheme exhibits linearity and realistic perturbation growth, except around the generation of clouds through large-scale condensation. Discontinuities and steep gradients are widely used here and severe problems occur in the calculation of cloud fraction. For data assimilation applications this poor behavior is controlled by replacing this part of the scheme with a perturbation model. For observation impacts, where efficiency is less of a concern, a filtering is developed that examines the Jacobian. The replacement scheme is only invoked if Jacobian elements or eigenvalues violate a series of tuned constants. The linearized prognostic cloud scheme is tested by comparing the linear and nonlinear perturbation trajectories for 6-, 12-, and 24-h forecast times. The tangent linear model performs well and perturbations of clouds are well captured for the lead times of interest.
C1 [Holdaway, Daniel; Errico, Ronald; Gelaro, Ronald; Kim, Jong G.; Mahajan, Rahul] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Holdaway, Daniel] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Errico, Ronald] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA.
[Kim, Jong G.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Mahajan, Rahul] Oak Ridge Associated Univ, NASA Postdoctoral Program, Oak Ridge, TN USA.
RP Holdaway, D (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, 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
FU NASA-USRA GESTAR
FX This work is funded under the NASA-USRA GESTAR cooperative agreement.
Thanks to Andrea Molod of GMAO for assistance in deciphering the cloud
model code.
NR 36
TC 0
Z9 0
U1 1
U2 1
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 OCT
PY 2015
VL 143
IS 10
BP 4198
EP 4219
DI 10.1175/MWR-D-15-0037.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CS6VK
UT WOS:000362220800020
ER
PT J
AU Ramsey, E
Rangoonwala, A
Jones, CE
Bannister, T
AF Ramsey, Elijah, III
Rangoonwala, Amina
Jones, Cathleen E.
Bannister, Terri
TI Maresh Canopy Leaf Area and Orientation Calculated for Improved Marsh
Structure Mapping
SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING
LA English
DT Article
ID PLANT-COMMUNITIES; INDEX; REFLECTANCE; VEGETATION; GRASSLAND; LIGHT;
RED; LOUISIANA; SPECTRA; DIEBACK
AB An approach is presented for producing the spatiotemporal estimation of leaf area index (LAI) of a highly heterogeneous coastal marsh without reliance on user estimates of marsh leaf-stem orientation. The canopy LAI profile derivation used three years of field measured photosynthetically active radiation (PAR) vertical profiles at seven S. alterniflora marsh sites and iterative transform of those PAR attenuation profiles to best-fit light extinction coefficients (KM). KM sun zenith dependency was removed obtaining the leaf angle distribution (LAD) representing the average marsh orientation and the LAD used to calculate the LAI canopy profile. LAI and LAD reproduced measured PAR profiles with 99 percent accuracy and corresponded to field documented structures. LAI and LAD better reflect marsh structure and results substantiate the need to account for marsh orientation. The structure indexes are directly amenable to remote sensing spatiotemporal mapping and offer a more meaningful representation of wetland systems promoting biophysical function understanding.
C1 [Ramsey, Elijah, III; Rangoonwala, Amina] US Geol Survey, Wetland & Aquat Res Ctr, Lafayette, LA 70506 USA.
[Jones, Cathleen E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bannister, Terri] Univ SW Louisiana, Reg Applicat Ctr, Lafayette, LA 70504 USA.
RP Ramsey, E (reprint author), US Geol Survey, Wetland & Aquat Res Ctr, 700 Cajundome Blvd, Lafayette, LA 70506 USA.
EM ramseye@usgs.gov
FU National Aeronautics Space Administration (NASA) [11-TE11-104]; US
Geological Survey Hurricane Sandy Supplemental Fund
FX We thank Dr. Stephen McNeill of Landcare Research Informatics Team for
his insightful and constructive review. This research was supported in
part by the National Aeronautics Space Administration (NASA) Grant No.
11-TE11-104 and was carried out in collaboration with the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA, and by US Geological Survey Hurricane Sandy Supplemental Funds.
Any use of trade, firm, or product names is for descriptive purposes
only and does not imply endorsement by the US Government.
NR 56
TC 2
Z9 2
U1 1
U2 7
PU AMER SOC PHOTOGRAMMETRY
PI BETHESDA
PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA
SN 0099-1112
J9 PHOTOGRAMM ENG REM S
JI Photogramm. Eng. Remote Sens.
PD OCT
PY 2015
VL 81
IS 10
BP 807
EP 816
PG 10
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
Photographic Technology
GA CS9DJ
UT WOS:000362389000006
ER
PT J
AU Kragh-Buetow, KC
Okojie, RS
Lukco, D
Mohney, SE
AF Kragh-Buetow, K. C.
Okojie, R. S.
Lukco, D.
Mohney, S. E.
TI Characterization of tungsten-nickel simultaneous Ohmic contacts to p-
and n-type 4H-SiC
SO SEMICONDUCTOR SCIENCE AND TECHNOLOGY
LA English
DT Article
DE 4H-SiC; Ohmic contact; tungsten; nickel; x-ray diffraction; Auger
electron spectroscopy
ID SILICON-CARBIDE; THERMAL-STABILITY; 4H-SILICON CARBIDE; ALLOYS; SYSTEM
AB Ohmic contacts to p-and n-type 4H-SiC using refractory alloyed W:Ni thin films were investigated. Transfer length measurement test structures to p-type 4H-SiC (N-A = 3 x 10(20) cm(-3)) revealed Ohmic contacts with specific contact resistances, rho(c), of similar to 10(-5) Omega cm(2) after 0.5 h annealing in argon at temperatures of 1000 degrees C, 1100 degrees C, 1150 degrees C, and 1200 degrees C. Contacts fabricated on n-type 4H-SiC (N-D = 2 x 10(19) cm(-3)) by similar methods were shown to have similar specific contact resistance values after annealing, demonstrating simultaneous Ohmic contact formation for W:Ni alloys on 4H-SiC. The lowest rho(c) values were (7.3 +/- 0.9) x 10(-6) Omega cm(2) for p-SiC and (6.8 +/- 3.1) x 10(-6) Omega cm(2) for n-SiC after annealing at 1150 degrees C. X-ray diffraction shows a cubic tungsten-nickel-carbide phase in the Ohmic contacts after annealing as well as WC after higher temperatures. Auger electron spectroscopy depth profiles support the presence of metal carbide regions above a nickel and silicon-rich region near the interface. X-ray energy dispersive spectroscopy mapping showed tungsten-rich and nickel-rich regions after annealing at 1100 degrees C and above. W: Ni alloys show promise as simultaneous Ohmic contacts to p- and n-SiC, offering low and comparable rho(c) values along with the formation of WxNiyC.
C1 [Kragh-Buetow, K. C.; Mohney, S. E.] Penn State Univ, Dept Mat Sci & Engn, University Pk, PA 16802 USA.
[Kragh-Buetow, K. C.; Mohney, S. E.] Penn State Univ, Mat Res Inst, University Pk, PA 16802 USA.
[Okojie, R. S.] NASA Glenn Res Ctr, Cleveland, OH USA.
[Lukco, D.] Vantage Partners LLC, Cleveland, OH USA.
RP Kragh-Buetow, KC (reprint author), Penn State Univ, Dept Mat Sci & Engn, University Pk, PA 16802 USA.
EM sem2@psu.edu
FU NASA Space Technology Research Fellowship (NSTRF) [NNX11AN03H]
FX The assistance and advice of Chuck Blaha, Jose M. Gonzalez, Kimala
Laster, Kelley Moses, Ariana Miller, Michelle Mrdenovich-Hill, Dr Phil
Neudeck, Beth Osborn, and David Spry at NASA Glenn Research Center is
greatly appreciated. Nichole Wonderling, Dr Trevor Clark, and Julie
Anderson in the Penn State Materials Characterization Laboratory are
also thanked for their assistance as well as Dr Amir Avishai at Case
Western Reserve University. K C Kragh-Buetow and this research
appreciate support from the NASA Space Technology Research Fellowship
(NSTRF) Grant #NNX11AN03H.
NR 45
TC 2
Z9 2
U1 6
U2 20
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0268-1242
EI 1361-6641
J9 SEMICOND SCI TECH
JI Semicond. Sci. Technol.
PD OCT
PY 2015
VL 30
IS 10
AR 105019
DI 10.1088/0268-1242/30/10/105019
PG 9
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA CT1ZR
UT WOS:000362602300027
ER
PT J
AU Wang, SH
Welton, EJ
Holben, BN
Tsay, SC
Lin, NH
Giles, D
Stewart, SA
Janjai, S
Nguyen, XA
Hsiao, TC
Chen, WN
Lin, TH
Buntoung, S
Chantara, S
Wiriya, W
AF Wang, Sheng-Hsiang
Welton, Ellsworth J.
Holben, Brent N.
Tsay, Si-Chee
Lin, Neng-Huei
Giles, David
Stewart, Sebastian A.
Janjai, Serm
Xuan Anh Nguyen
Hsiao, Ta-Chih
Chen, Wei-Nai
Lin, Tang-Huang
Buntoung, Sumaman
Chantara, Somporn
Wiriya, Wan
TI Vertical Distribution and Columnar Optical Properties of Springtime
Biomass-Burning Aerosols over Northern Indochina during 2014 7-SEAS
Campaign
SO AEROSOL AND AIR QUALITY RESEARCH
LA English
DT Article
DE Aerosol optical properties; Smoke haze; Biomass burning; Lidar; Seven
South East Asian Studies (7-SEAS)
ID SKY RADIANCE MEASUREMENTS; SOUTHEAST-ASIA; 7-SEAS/DONGSHA EXPERIMENT;
BASE-ASIA; AERONET; VARIABILITY; SATELLITE; AFRICA; CLOUDS; SEASON
AB In this study, the aerosol optical properties and vertical distributions in major biomass-burning emission area of northern Indochina were investigated using ground-based remote sensing (i.e., four Sun-sky radiometers and one lidar) during the Seven South East Asian Studies/Biomass-burning Aerosols & Stratocumulus Environment: Lifecycles & Interactions Experiment conducted during spring 2014. Despite the high spatial variability of the aerosol optical depth (AOD; which at 500 nm ranged from 0.75 to 1.37 depending on the site), the temporal variation of the daily AOD demonstrated a consistent pattern among the observed sites, suggesting the presence of widespread smoke haze over the region. Smoke particles were characterized as small (Angstrom exponent at 440-870 nm of 1.72 and fine mode fraction of 0.96), strongly absorbing (single-scattering albedo at 440 nm of 0.88), mixture of black and brown carbon particles (absorption Angstrom exponent at 440-870 nm of 1.5) suspended within the planetary boundary layer (PBL). Smoke plumes driven by the PBL dynamics in the mountainous region reached as high as 5 km above sea level; these plumes subsequently spread out by westerly winds over northern Vietnam, southern China, and the neighboring South China Sea. Moreover, the analysis of diurnal variability of aerosol loading and optical properties as well as vertical profile in relation to PBL development, fire intensity, and aerosol mixing showed that various sites exhibited different variability based on meteorological conditions, fuel type, site elevation, and proximity to biomass-burning sources. These local factors influence the aerosol characteristics in the region and distinguish northern Indochina smoke from other biomass-burning regions in the world.
C1 [Wang, Sheng-Hsiang; Lin, Neng-Huei] Natl Cent Univ, Dept Atmospher Sci, Taoyuan, Taiwan.
[Welton, Ellsworth J.; Holben, Brent N.; Tsay, Si-Chee; Giles, David; Stewart, Sebastian A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Giles, David; Stewart, Sebastian A.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Janjai, Serm; Buntoung, Sumaman] Silpakorn Univ, Dept Phys, Fac Sci, Nakhon Pathom, Thailand.
[Xuan Anh Nguyen] Vietnam Acad Sci & Technol, Inst Geophys, Hanoi, Vietnam.
[Hsiao, Ta-Chih] Natl Cent Univ, Grad Inst Environm Engn, Taoyuan, Taiwan.
[Chen, Wei-Nai] Acad Sinica, Res Ctr Environm Changes, Taipei 115, Taiwan.
[Lin, Tang-Huang] Natl Cent Univ, Ctr Space & Remote Sensing Res, Taoyuan, Taiwan.
[Chantara, Somporn; Wiriya, Wan] Chiang Mai Univ, Fac Sci, Dept Chem, Chiang Mai 50000, Thailand.
[Chantara, Somporn; Wiriya, Wan] Chiang Mai Univ, Fac Sci, Environm Sci Program, Chiang Mai 50000, Thailand.
RP Wang, SH (reprint author), Natl Cent Univ, Dept Atmospher Sci, Taoyuan, Taiwan.
EM shenghsiang.wang@gmail.com
RI Wang, Sheng-Hsiang/F-4532-2010
OI Wang, Sheng-Hsiang/0000-0001-9675-3135
FU National Science Council of Taiwan [MOST 103-2111-M-008-006,
101-2119-M-008-012]; Taiwan EPA [EPA-103-U1L1-02-101]; NASA
FX This work was supported by the National Science Council of Taiwan under
grants No. MOST 103-2111-M-008-006, 101-2119-M-008-012 and by the Taiwan
EPA under contracts No. EPA-103-U1L1-02-101. The 7-SEAS, AERONET,
MPLNET, project was supported by the NASA Radiation Sciences Program
managed by Dr. Hal Maring. The authors thank the AERONET team for
calibrating and maintaining instrumentation and processing these data.
Thanks are also given to all assistants and graduate students involving
in the site operation, data analysis and technical support for making
7-SEAS/BASELInE campaign successful.
NR 47
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U1 1
U2 17
PU TAIWAN ASSOC AEROSOL RES-TAAR
PI TAICHUNG COUNTY
PA CHAOYANG UNIV TECH, DEPT ENV ENG & MGMT, PROD CTR AAQR, NO 168, JIFONG E
RD, WUFONG TOWNSHIP, TAICHUNG COUNTY, 41349, TAIWAN
SN 1680-8584
EI 2071-1409
J9 AEROSOL AIR QUAL RES
JI Aerosol Air Qual. Res.
PD OCT
PY 2015
VL 15
IS 5
BP 2037
EP 2050
DI 10.4209/aaqr.2015.05.0310
PG 14
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA CS3KC
UT WOS:000361971500028
ER
PT J
AU Blickensderfer, EL
Lanicci, JM
Vincent, MJ
Thomas, RL
Smith, M
Cruit, JK
AF Blickensderfer, Elizabeth L.
Lanicci, John M.
Vincent, Michael J.
Thomas, Robert L.
Smith, MaryJo
Cruit, Jessica K.
TI Training General Aviation Pilots for Convective Weather Situations
SO AEROSPACE MEDICINE AND HUMAN PERFORMANCE
LA English
DT Article
DE aviation weather; NEXRAD; training
ID SELF-EFFICACY; EXPERT
AB BACKGROUND: Over the past 10-15 yr, considerable research has occurred for the development, testing, and fielding of real-time Datalink weather products for general aviation (GA) pilots to use before and during flight. As is the case with the implementation of most new technologies, work is needed to ensure that the users (in this case, the pilots) understand both the capabilities and limitations of the new technologies as well as how to use the new systems to improve their task performance. The purpose of this study was to replicate and extend a previous study on training pilots how and when to use these new weather technologies.
METHOD: This field study used a quasi-experimental design (pre- vs. post-test with a control group). There were 91 GA pilots from the Midwest, Northeastern, and Southeastern United States who participated in a 2-h short course or a control activity. The lecture-based short course covered radar basics, Next Generation Weather Radar (NEXRAD), NEXRAD specifics/limitations, thunderstorm basics, radar products, and decision making.
RESULTS: The pilots who participated in the course earned higher knowledge test scores, improved at applying the concepts in paper-based flight scenarios, had higher self-efficacy in post-training assessments as compared to pre-training assessments, and also performed better than did control subjects on post-test knowledge and skills assessments.
DISCUSSION: GA pilots lack knowledge about real-time Datalink weather technology. This study indicates that a relatively short training program was effective for fostering Datalink weather-related knowledge and skills in GA pilots.
C1 [Smith, MaryJo; Cruit, Jessica K.] Embry Riddle Aeronaut Univ, Daytona Beach, FL 32114 USA.
[Blickensderfer, Elizabeth L.] Human Factors Dept, Daytona Beach, FL USA.
[Lanicci, John M.] Dept Grad Studies, Daytona Beach, FL USA.
[Thomas, Robert L.] Aeronaut Sci Dept, Daytona Beach, FL USA.
[Vincent, Michael J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Blickensderfer, EL (reprint author), Embry Riddle Aeronaut Univ, Human Factors Dept, 600 S Clyde Morris Blvd, Daytona Beach, FL 32114 USA.
EM blick488@erau.edu
FU Federal Aviation Administration's (FAA) Center for Excellence in General
Aviation Research under FAA Cooperative Agreement [07-C-GA-ERAU-014]
FX This research was conducted under sponsorship of the Federal Aviation
Administration's (FAA) Center for Excellence in General Aviation
Research under FAA Cooperative Agreement Number 07-C-GA-ERAU-014.
NR 20
TC 0
Z9 0
U1 4
U2 8
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 2375-6314
EI 2375-6322
J9 AEROSP MED HUM PERF
JI Aerosp. Med.Hum. Perform.
PD OCT
PY 2015
VL 86
IS 10
BP 881
EP 888
DI 10.3357/AMHP.4174.2015
PG 8
WC Biophysics; Public, Environmental & Occupational Health; Medicine,
Research & Experimental
SC Biophysics; Public, Environmental & Occupational Health; Research &
Experimental Medicine
GA CS4PF
UT WOS:000362057300005
PM 26564675
ER
PT J
AU Bahadori, A
Miglioretti, D
Kruger, R
Flynn, M
Weinmann, S
Smith-Bindman, R
Lee, C
AF Bahadori, Amir
Miglioretti, Diana
Kruger, Randell
Flynn, Michael
Weinmann, Sheila
Smith-Bindman, Rebecca
Lee, Choonsik
TI Calculation of Organ Doses for a Large Number of Patients Undergoing CT
Examinations
SO AMERICAN JOURNAL OF ROENTGENOLOGY
LA English
DT Article
DE CT; dosimetry; informatics; Monte Carlo simulations; phantom
ID COMPUTED-TOMOGRAPHY; RADIATION-EXPOSURE; PEDIATRIC CT; CANCER-RISK;
DOSIMETRY; SCANS; POPULATION; PHANTOMS; CHILDREN; PROGRAM
AB OBJECTIVE. The objective of our study was to develop an automated calculation method to provide organ dose assessment for a large cohort of pediatric and adult patients undergoing CT examinations.
MATERIALS AND METHODS. We adopted two dose libraries that were previously published: the volume CT dose index-normalized organ dose library and the tube current-exposure time product (100 mAs)-normalized weighted CT dose index library. We developed an algorithm to calculate organ doses using the two dose libraries and the CT parameters available from DICOM data. We calculated organ doses for pediatric (n = 2499) and adult (n = 2043) CT examinations randomly selected from four health care systems in the United States and compared the adult organ doses with the values calculated from the ImPACT calculator.
RESULTS. The median brain dose was 20 mGy (pediatric) and 24 mGy (adult), and the brain dose was greater than 40 mGy for 11% (pediatric) and 18% (adult) of the head CT studies. Both the National Cancer Institute (NCI) and ImPACT methods provided similar organ doses (median discrepancy < 20%) for all organs except the organs located close to the scanning boundaries. The visual comparisons of scanning coverage and phantom anatomies revealed that the NCI method, which is based on realistic computational phantoms, provides more accurate organ doses than the ImPACT method.
CONCLUSION. The automated organ dose calculation method developed in this study reduces the time needed to calculate doses for a large number of patients. We have successfully used this method for a variety of CT-related studies including retrospective epidemiologic studies and CT dose trend analysis studies.
C1 [Bahadori, Amir] NASA, Space Radiat Anal Grp, Johnson Space Ctr, Houston, TX USA.
[Miglioretti, Diana] Univ Calif Davis, Sch Med, Dept Publ Hlth Sci, Div Biostat, Davis, CA 95616 USA.
[Kruger, Randell] Marshfield Clin & Res Fdn, Dept Radiol, Marshfield, WI USA.
[Flynn, Michael] Henry Ford Hlth Syst, Dept Radiol, Detroit, MI USA.
[Flynn, Michael] Henry Ford Hlth Syst, Ctr Hlth Serv Res, Detroit, MI USA.
[Weinmann, Sheila] Kaiser Permanente Northwest, Ctr Hlth Res, Portland, OR USA.
[Smith-Bindman, Rebecca] Univ Calif San Francisco, Dept Radiol & Biomed Imaging, San Francisco, CA 94143 USA.
[Smith-Bindman, Rebecca] Univ Calif San Francisco, Dept Epidemiol & Biostat, San Francisco, CA 94143 USA.
[Smith-Bindman, Rebecca] Univ Calif San Francisco, Dept Obstet Gynecol & Reprod Sci, San Francisco, CA USA.
[Lee, Choonsik] NCI, Div Canc Epidemiol & Genet, Radiat Epidemiol Branch, NIH, Rockville, MD 20850 USA.
RP Lee, C (reprint author), NCI, Div Canc Epidemiol & Genet, Radiat Epidemiol Branch, NIH, 9609 Med Ctr Dr, Rockville, MD 20850 USA.
EM leechoonsik@mail.nih.gov
RI Lee, Choonsik/C-9023-2015
OI Lee, Choonsik/0000-0003-4289-9870
FU National Institutes of Health, National Cancer Institute, Division of
Cancer Epidemiology and Genetics
FX This work was supported by the intramural research program of the
National Institutes of Health, National Cancer Institute, Division of
Cancer Epidemiology and Genetics.
NR 24
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Z9 0
U1 0
U2 1
PU AMER ROENTGEN RAY SOC
PI RESTON
PA 1891 PRESTON WHITE DR, SUBSCRIPTION FULFILLMENT, RESTON, VA 22091 USA
SN 0361-803X
EI 1546-3141
J9 AM J ROENTGENOL
JI Am. J. Roentgenol.
PD OCT
PY 2015
VL 205
IS 4
BP 827
EP 833
DI 10.2214/AJR.14.14135
PG 7
WC Radiology, Nuclear Medicine & Medical Imaging
SC Radiology, Nuclear Medicine & Medical Imaging
GA CS1SF
UT WOS:000361847300034
PM 26397332
ER
PT J
AU Zhang, Y
Kim, M
Guo, HG
Sunderland, PB
Quintiere, JG
deRis, J
Stocker, DP
AF Zhang, Yi
Kim, Matt
Guo, Haiging
Sunderland, Peter B.
Quintiere, James G.
deRis, John
Stocker, Dennis P.
TI Emulation of condensed fuel flames with gases in microgravity
SO COMBUSTION AND FLAME
LA English
DT Article
DE Diffusion flame; Fire; Heat flux; Microgravity
ID COMBUSTION; EXTINCTION
AB A gaseous fuel burner has been designed to emulate the burning behavior of liquids and solids. The burner is hypothesized to represent a liquid or solid fuel through four key properties: heat of combustion, heat of gasification, vaporization temperature, and laminar smoke point. Previous work supports this concept, and it has been demonstrated for four real fuels. The technique is applied to flames during 5 s of microgravity. Tests were conducted with a burner of 25 mm diameter, two gaseous fuels, and a range of flow rates, oxygen concentrations, and pressures. The microgravity tests reveal a condition appearing to approach a steady state but sometimes with apparent local extinction. The flame typically retains a hemispherical shape, with some indication of slowing growth, and nearly asymptotic steady flame heat flux. A one-dimensional steady-state theory reasonably correlates the data for flame heat flux and flame length. The burning rate per unit area is found to be inversely dependent on diameter and a function of the ratio of the ambient oxygen mass fraction to the heat of gasification. The flame length to diameter ratio depends on two dimensionless parameters: Spalding B number and the ratio of the heat of combustion per unit mass of ambient oxygen to the heat of combustion of the fuel mixture stream. (C) 2015 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Zhang, Yi; Kim, Matt; Guo, Haiging; Sunderland, Peter B.; Quintiere, James G.] Univ Maryland, Dept Fire Protect Engn, College Pk, MD 20742 USA.
[deRis, John] FM Global, Johnston, IA USA.
[Stocker, Dennis P.] NASA, Glenn Res Ctr, New York, NY USA.
RP Quintiere, JG (reprint author), Univ Maryland, Dept Fire Protect Engn, 3104 JM Patterson Bldg, College Pk, MD 20742 USA.
EM jimq@umd.edu
OI Sunderland, Peter/0000-0002-8262-7100
FU NASA [NNX10AD98G]
FX We are indebted to invaluable support from NASA, namely technical input
from Paul V. Ferkul and Fumiaki Takahashi, and Jay Owens and the
microgravity tests directed by Eric Neumann. This study was supported by
NASA grant NNX10AD98G.
NR 22
TC 1
Z9 2
U1 1
U2 6
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 OCT
PY 2015
VL 162
IS 10
BP 3449
EP 3455
DI 10.1016/j.combustflame.2015.05.005
PG 7
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA CS2TT
UT WOS:000361925600002
ER
PT J
AU Ehsan, N
Hsieh, WT
Moseley, SH
Wollack, EJ
AF Ehsan, Negar
Hsieh, Wen-Ting
Moseley, Samuel H.
Wollack, Edward J.
TI Broadband Planar 5:1 Impedance Transformer
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE Broadband; impedance matching; parallel-plate line; transformers
ID TRANSMISSION-LINE TRANSFORMERS; NETWORKS; DESIGN
AB This letter presents a broadband Guanella-type planar impedance transformer that transforms 50 Omega to 10 Omega with a 10 dB bandwidth of 1-14 GHz. The transformer is designed on a flexible 50 mu m thick polyimide substrate in microstrip and parallel-plate transmission line topologies, and is inspired by the traditional 4: 1 Guanella transformer. Back-to-back transformers were designed and fabricated for characterization in a 50 Omega system. Simulated and measured results are in excellent agreement.
C1 [Ehsan, Negar; Hsieh, Wen-Ting; Moseley, Samuel H.; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ehsan, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM negar.ehsan@nasa.gov
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
NR 14
TC 1
Z9 1
U1 0
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1531-1309
EI 1558-1764
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD OCT
PY 2015
VL 25
IS 10
BP 636
EP 638
DI 10.1109/LMWC.2015.2463106
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA CS8SP
UT WOS:000362359100002
ER
PT J
AU Song, P
Oakley, MA
Ulusoy, AC
Kaynak, M
Tillack, B
Sadowy, GA
Cressler, JD
AF Song, Peter
Oakley, Michael A.
Ulusoy, A. Cagri
Kaynak, Mehmet
Tillack, Bernd
Sadowy, Gregory A.
Cressler, John D.
TI A Class-E Tuned W-Band SiGe Power Amplifier With 40.4% Power-Added
Efficiency at 93 GHz
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE Millimeter wave integrated circuits (mm-wave IC); power amplifiers (PA);
silicon germanium (SiGe)
ID CMOS
AB A W-band power amplifier with Class-E tuning in a 0.13 mu m SiGe BiCMOS technology is presented. Voltage swing beyond BVCBO is enabled by the cascode topology, low upper base resistance, and minimally overlapping current-voltage waveforms. At 93 GHz with 4.0 V bias, the peak power-added efficiency and saturated output power are measured to be 40.4% and 17.7 dBm, respectively. With the bias increased to 5.2 V, the peak power-added efficiency and saturated output power at 93 GHz are measured to be 37.6% and 19.3 dBm, respectively.
C1 [Song, Peter; Oakley, Michael A.; Cressler, John D.] Sch Elect & Comp Engn, Atlanta, GA 30332 USA.
[Ulusoy, A. Cagri; Kaynak, Mehmet; Tillack, Bernd] IHP Microelect GmbH, D-15236 Frankfurt, Oder, Germany.
[Tillack, Bernd] Tech Univ Berlin, D-10587 Berlin, Germany.
[Sadowy, Gregory A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Song, P (reprint author), Sch Elect & Comp Engn, Atlanta, GA 30332 USA.
EM songp@gatech.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 11
TC 4
Z9 4
U1 0
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1531-1309
EI 1558-1764
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD OCT
PY 2015
VL 25
IS 10
BP 663
EP 665
DI 10.1109/LMWC.2015.2463231
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA CS8SP
UT WOS:000362359100011
ER
PT J
AU Tawfik, AB
Dirmeyer, PA
Santanello, JA
AF Tawfik, Ahmed B.
Dirmeyer, Paul A.
Santanello, Joseph A., Jr.
TI The Heated Condensation Framework. Part I: Description and Southern
Great Plains Case Study
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Boundary layer; Convective clouds; Atmosphere-land interaction;
Convective-scale processes; Hydrometeorology; Surface fluxes
ID ATMOSPHERE COUPLING EXPERIMENT; 12 JUNE 2002; PRECONDITIONING DEEP
CONVECTION; BOUNDARY LAYER INTERACTIONS; DIURNAL-CYCLE; SOIL-MOISTURE;
UNITED-STATES; CUMULUS CONGESTUS; CLIMATE MODELS; NORTH-AMERICA
AB This study extends the heated condensation framework (HCF) presented in Tawfik and Dirmeyer to include variables for describing the convective background state of the atmosphere used to quantify the contribution of the atmosphere to convective initiation within the context of land-atmosphere coupling. In particular, the ability for the full suite of HCF variables to 1) quantify the amount of latent and sensible heat energy necessary for convective initiation, 2) identify the transition from moistening advantage to boundary layer growth advantage, 3) identify locally originating convection, and 4) compare models and observations, directly highlighting biases in the convective state, is demonstrated. These capabilities are illustrated for a clear-sky and convectively active day over the Atmospheric Radiation Measurement Program Southern Great Plains central station using observations, the Rapid Update Cycle (RUC) operational model, and the North American Regional Reanalysis (NARR). The clear-sky day had a higher and unattainable convective threshold, making convective initiation unlikely. The convectively active day had a lower threshold that was attained by midafternoon, reflecting local convective triggering. Compared to observations, RUC tended to have the most difficulty representing the convective state and captured the threshold for the clear-sky case only because of compensating biases in the moisture and temperature profiles. Despite capturing the observed moisture profile very well, a stronger surface inversion in NARR returned overestimates in the convective threshold. The companion paper applies the HCF variables introduced here across the continental United States to examine the climatological behavior of convective initiation and local land-atmosphere coupling.
C1 [Tawfik, Ahmed B.; Dirmeyer, Paul A.] George Mason Univ, Ctr Ocean Land Atmosphere Studies, Fairfax, VA 22030 USA.
[Santanello, Joseph A., Jr.] NASA, Goddard Space Flight Ctr, Hydrol Sci, Greenbelt, MD 20771 USA.
RP Tawfik, AB (reprint author), Natl Ctr Atmospher Res, Climate & Global Dynam, 1850 Table Mesa Dr, Boulder, CO 80305 USA.
EM abtawfik@ucar.edu
RI Dirmeyer, Paul/B-6553-2016; Tawfik, Ahmed/D-3683-2015; Santanello,
Joseph/D-4438-2012
OI Dirmeyer, Paul/0000-0003-3158-1752; Tawfik, Ahmed/0000-0002-6631-9300;
Santanello, Joseph/0000-0002-0807-6590
FU National Science Foundation [0947837]
FX This work was supported by National Science Foundation Grant 0947837 for
Earth System Modeling postdoctoral fellows. We thank Chiel van
Heerwaarden for his excellent review and feedback, which greatly
improved the methodology and quality of the manuscript.
NR 80
TC 5
Z9 5
U1 1
U2 12
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD OCT
PY 2015
VL 16
IS 5
BP 1929
EP 1945
DI 10.1175/JHM-D-14-0117.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CS6VZ
UT WOS:000362222500001
ER
PT J
AU Tawfik, AB
Dirmeyer, PA
Santanello, JA
AF Tawfik, Ahmed B.
Dirmeyer, Paul A.
Santanello, Joseph A., Jr.
TI The Heated Condensation Framework. Part II: Climatological Behavior of
Convective Initiation and Land-Atmosphere Coupling over the Conterminous
United States
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Convection; Boundary layer; Convective clouds; Atmosphere-land
interaction; Convective-scale processes; Soil moisture
ID MOISTURE-PRECIPITATION FEEDBACK; BOUNDARY LAYER INTERACTIONS; SOUTHERN
GREAT-PLAINS; SOIL-MOISTURE; CLOUD DEVELOPMENT; NORTH-AMERICA; SURFACE;
REANALYSIS; SIMULATIONS; EVAPORATION
AB This is Part II of a two-part study introducing the heated condensation framework (HCF), which quantifies the potential convective state of the atmosphere in terms of land-atmosphere interactions. Part I introduced the full suite of HCF variables and applied them to case studies with observations and models over a single location in the southern Great Plains. It was shown in Part I that the HCF was capable of identifying locally initiated convection and quantifying energetically favorable pathways for initiation. Here, the HCF is applied to the entire conterminous United States and the climatology of convective initiation (CI) in relation to local land-atmosphere coupling (LoCo) is explored for 34 summers (June-August) using the North American Regional Reanalysis (NARR) and observations. NARR is found to be capable of capturing the convective threshold (buoyant mixing potential temperature (BM)) and energy advantage transition (energy advantage potential temperature (adv)) for most of the United States. However, there are compensating biases in the components of moisture q(mix) and temperature q*, resulting in low (BM) biases for the wrong reason. The HCF has been used to show that local CI occurred over the Rocky Mountains and the southern Great Plains 35%-65% of the time. Finally, the LoCo process chain has been recast in light of the HCF. Both positive and negative soil moisture-convective feedbacks are possible, with negative feedbacks producing a stronger response in CI likelihood under weak convective inhibition. Positive feedbacks are present but weaker.
C1 [Tawfik, Ahmed B.; Dirmeyer, Paul A.] George Mason Univ, Ctr Ocean Land Atmosphere Studies, Fairfax, VA 22030 USA.
[Santanello, Joseph A., Jr.] NASA, Goddard Space Flight Ctr, Hydrol Sci, Greenbelt, MD 20771 USA.
RP Tawfik, AB (reprint author), Natl Ctr Atmospher Res, Climate & Global Dynam, 1850 Table Mesa Dr, Boulder, CO 80305 USA.
EM abtawfik@ucar.edu
RI Dirmeyer, Paul/B-6553-2016; Tawfik, Ahmed/D-3683-2015; Santanello,
Joseph/D-4438-2012
OI Dirmeyer, Paul/0000-0003-3158-1752; Tawfik, Ahmed/0000-0002-6631-9300;
Santanello, Joseph/0000-0002-0807-6590
FU National Science Foundation [0947837]
FX This work was supported by National Science Foundation Grant 0947837 for
Earth System Modeling postdocs. We thank Chiel van Heerwaarden for his
excellent review and feedback regarding the methodology and Craig
Ferguson for the early discussion that aided in the development of a
portion of this work.
NR 42
TC 5
Z9 5
U1 2
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD OCT
PY 2015
VL 16
IS 5
BP 1946
EP 1961
DI 10.1175/JHM-D-14-0118.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CS6VZ
UT WOS:000362222500002
ER
PT J
AU Beauchamp, RM
Chandrasekar, V
Chen, HN
Vega, M
AF Beauchamp, Robert M.
Chandrasekar, V.
Chen, Haonan
Vega, Manuel
TI Overview of the D3R Observations during the IFloodS Field Experiment
with Emphasis on Rainfall Mapping and Microphysics
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
DE Radars; Radar observations
ID RADAR
AB The NASA dual-frequency, dual-polarization Doppler radar (D3R) was deployed as part of the GPM Iowa Flood Studies (IFloodS) ground validation field campaign from 1 May through 15 June 2013. The D3R participated in a multi-instrument targeted investigation of convective initiation and hydrological response in the midwestern United States. An overview of the D3R's calibration and observations is presented. A method for attenuation correction of Ka-band observations using Ku-band results is introduced. Dual-frequency ratio estimates in stratiform rain and ice are presented and compared with theoretical values. Ku-band quantitative precipitation estimation results are validated against IFloodS ground instruments.
C1 [Beauchamp, Robert M.; Chandrasekar, V.; Chen, Haonan; Vega, Manuel] Colorado State Univ, Ft Collins, CO 80523 USA.
[Vega, Manuel] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Chandrasekar, V (reprint author), Colorado State Univ, 1373 Campus Delivery, Ft Collins, CO 80523 USA.
EM chandra@engr.colostate.edu
RI Measurement, Global/C-4698-2015;
OI Chen, Haonan/0000-0002-9795-3064
FU GPM program
FX The authors acknowledge the support of the GPM program, David Wolff and
David Marks for NPOL support, and Mathew Schwaller and Walter Petersen
for deployment and logistics support. In addition, the authors
acknowledge all the participants of the IFloodS field campaign.
NR 12
TC 1
Z9 1
U1 0
U2 5
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 OCT
PY 2015
VL 16
IS 5
BP 2118
EP 2132
DI 10.1175/JHM-D-15-0023.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CS6VZ
UT WOS:000362222500012
ER
PT J
AU Liu, YD
Sander, SP
AF Liu, Yingdi
Sander, Stanley P.
TI Rate Constant for the OH plus CO Reaction at Low Temperatures
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID PRESSURE-DEPENDENCE; GAS-PHASE; MARTIAN ATMOSPHERE; RADICALS; KINETICS;
HO
AB Rate constants for the reaction of OH + CO -> products (1) have been measured using laser photolysis/laser-induced fluorescence (LP/LIF) over the temperature range 193-296 K and at pressures of 50-700 Torr of Ar and N-2. The reaction was studied under pseudo-first-order conditions, monitoring the decay of OH in the presence of a large excess of CO. The rate constants can be expressed as a combination of bimolecular and termolecular components. The bimolecular component was found to be temperature-independent with an expression given by k(bi)(T) = (1.54 +/- 0.14) x 10(-13)[e(-(13)+/-(17)/T)] cm(3) molecule(-1) s(-1), with an error of one standard deviation. The termolecular component was fitted to the expression, k(ter) = k(0)(T)[M]/[1 + (k(0)(T)[M]/k(infinity)(T)] x 0.6(10)({1+[log)((k0(T)[M]/k infinity(T))]2}-1) where k(0)(T) = k(0)(300)(T/300)(-n) and k(infinity)(T) = k(infinity)(300)(T/300)(-m). The parameters for k(0)(T) were determined to be k(0)(300) = (6.0 +/- 0.5) X 10(-33) cm(6) molecule(-2) s(-1) in N-2 and k(0)(300) = (3.4 +/- 0.3) x 10(-33) cm(6) molecule(-2) s(-1) in Ar, with n = 1.9 +/- 0.5 and 2.0 +/- 0.4 in N-2 and Ar, respectively. These parameters were determined using k(0)(T) and m from the NASA kinetics data evaluation (JPL Publication No. 10-6) since the experimental pressure range was far from the high-pressure limit. Addition of low concentrations of O-2 had no discernible effect on the mechanism of the OH + CO reaction but resulted in secondary reactions which regenerated OH.
C1 [Liu, Yingdi; Sander, Stanley P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sander, SP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Stanley.P.Sander@jpl.nasa.gov
FU NASA Mars Fundamental Research, Upper Atmosphere Research and
Tropospheric Chemistry Programs
FX This work was supported by the NASA Mars Fundamental Research, Upper
Atmosphere Research and Tropospheric Chemistry Programs. The authors
thank A. Komissarov who carried out initial experimental studies,
members of the JPL Lab Studies and Modeling Group for helpful
discussions, and Dave Natzic for technical assistance. Copyright 2015,
California Institute of Technology.
NR 21
TC 2
Z9 2
U1 4
U2 15
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD OCT 1
PY 2015
VL 119
IS 39
BP 10060
EP 10066
DI 10.1021/acs.jpca.5b07220
PG 7
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA CS9BP
UT WOS:000362384400012
PM 26305192
ER
PT J
AU Stokes, CR
Tarasov, L
Blomdin, R
Cronin, TM
Fisher, TG
Gyllencreutz, R
Hattestrand, C
Heyman, J
Hindmarsh, RCA
Hughes, ALC
Jakobsson, M
Kirchner, N
Livingstone, SJ
Margold, M
Murton, JB
Riko, N
Peltier, WR
Peteet, DM
Piper, DJW
Preusser, F
Renssen, H
Roberts, DH
Roche, DM
Saint-Ange, F
Stroeven, AP
Teller, JT
AF Stokes, Chris R.
Tarasov, Lev
Blomdin, Robin
Cronin, Thomas M.
Fisher, Timothy G.
Gyllencreutz, Richard
Hattestrand, Clas
Heyman, Jakob
Hindmarsh, Richard C. A.
Hughes, Anna L. C.
Jakobsson, Martin
Kirchner, Nina
Livingstone, Stephen J.
Margold, Martin
Murton, Julian B.
Noormets, Riko
Peltier, W. Richard
Peteet, Dorothy M.
Piper, David J. W.
Preusser, Frank
Renssen, Hans
Roberts, David H.
Roche, Didier M.
Saint-Ange, Francky
Stroeven, Arjen P.
Teller, James T.
TI On the reconstruction of palaeo-ice sheets: Recent advances and future
challenges
SO QUATERNARY SCIENCE REVIEWS
LA English
DT Review
DE Ice sheet reconstruction; Numerical modelling; Palaeoglaciology;
Glaciology
ID LAST GLACIAL MAXIMUM; RELATIVE SEA-LEVEL; LATE QUATERNARY STRATIGRAPHY;
LARGE ENSEMBLE ANALYSIS; C-14 YR BP; COSMOGENIC NUCLIDE MEASUREMENTS;
MODEL INTERCOMPARISON PROJECT; CANADIAN ARCTIC ARCHIPELAGO;
PRODUCTION-RATE CALIBRATION; GROUNDING LINE MOTION
AB Reconstructing the growth and decay of palaeo-ice sheets is critical to understanding mechanisms of global climate change and associated sea-level fluctuations in the past, present and future. The significance of palaeo-ice sheets is further underlined by the broad range of disciplines concerned with reconstructing their behaviour, many of which have undergone a rapid expansion since the 1980s. In particular, there has been a major increase in the size and qualitative diversity of empirical data used to reconstruct and date ice sheets, and major improvements in our ability to simulate their dynamics in numerical ice sheet models. These developments have made it increasingly necessary to forge interdisciplinary links between sub-disciplines and to link numerical modelling with observations and dating of proxy records. The aim of this paper is to evaluate recent developments in the methods used to reconstruct ice sheets and outline some key challenges that remain, with an emphasis on how future work might integrate terrestrial and marine evidence together with numerical modelling. Our focus is on pan-ice sheet reconstructions of the last deglaciation, but regional case studies are used to illustrate methodological achievements, challenges and opportunities. Whilst various disciplines have made important progress in our understanding of ice-sheet dynamics, it is clear that data-model integration remains under-used, and that uncertainties remain poorly quantified in both empirically-based and numerical ice-Sheet reconstructions. The representation of past climate will continue to be the largest source of uncertainty for numerical modelling. As such, palaeo-observations are critical to constrain and validate modelling. State-of-the-art numerical models will continue to improve both in model resolution and in the breadth of inclusion of relevant processes, thereby enabling more accurate and more direct comparison with the increasing range of palaeo-observations. Thus, the capability is developing to use all relevant palaeo-records to more strongly constrain deglacial (and to a lesser extent pre-LGM) ice sheet evolution. In working towards that goal, the accurate representation of uncertainties is required for both constraint data and model outputs. Close cooperation between modelling and data-gathering communities is essential to ensure this capability is realised and continues to progress. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Stokes, Chris R.; Margold, Martin; Roberts, David H.] Univ Durham, Dept Geog, Durham DH1 3LE, England.
[Tarasov, Lev] Mem Univ Newfoundland, Dept Phys & Phys Oceanog, St John, NF A1B 3X7, Canada.
[Blomdin, Robin] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA.
[Blomdin, Robin; Hattestrand, Clas; Heyman, Jakob; Kirchner, Nina; Margold, Martin; Stroeven, Arjen P.] Stockholm Univ, Dept Phys Geog, S-10691 Stockholm, Sweden.
[Blomdin, Robin; Hattestrand, Clas; Heyman, Jakob; Kirchner, Nina; Margold, Martin; Stroeven, Arjen P.] Stockholm Univ, Bolin Ctr Climate Res, S-10691 Stockholm, Sweden.
[Cronin, Thomas M.] US Geol Survey, Reston, VA 20192 USA.
[Fisher, Timothy G.] Univ Toledo, Dept Environm Sci, Toledo, OH 43606 USA.
[Gyllencreutz, Richard; Jakobsson, Martin] Stockholm Univ, Dept Geol Sci, S-10691 Stockholm, Sweden.
[Hindmarsh, Richard C. A.] British Antarctic Survey, Cambridge CB3 0ET, England.
[Hughes, Anna L. C.] Univ Bergen, Dept Earth Sci, N-5007 Bergen, Norway.
[Hughes, Anna L. C.] Bjerknes Ctr Climate Res, N-5007 Bergen, Norway.
[Livingstone, Stephen J.] Univ Sheffield, Dept Geog, Sheffield S10 2TN, S Yorkshire, England.
[Murton, Julian B.] Univ Sussex, Dept Geog, Brighton BN1 9QJ, E Sussex, England.
[Noormets, Riko] Univ Ctr Svalbard UNIS, N-9171 Longyearbyen, Norway.
[Peltier, W. Richard] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Peteet, Dorothy M.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Peteet, Dorothy M.] NASA Goddard Inst Space Studies, New York, NY 10025 USA.
[Piper, David J. W.; Saint-Ange, Francky] Geol Survey Canada Atlantic, Bedford Inst Oceanog, Dartmouth, NS B2Y 4A2, Canada.
[Preusser, Frank] Univ Freiburg, Inst Earth & Environm Sci Geol, D-79104 Freiburg, Germany.
[Renssen, Hans; Roche, Didier M.] Vrije Univ Amsterdam, Fac Earth & Life Sci, Amsterdam, Netherlands.
[Roche, Didier M.] CEA CNRS INSU UVSQ, LSCE, Gif Sur Yvette, France.
[Teller, James T.] Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada.
RP Stokes, CR (reprint author), Univ Durham, Dept Geog, Durham DH1 3LE, England.
EM c.r.stokes@durham.ac.uk
RI Stokes, Chris/A-1957-2011; Peltier, William/A-1102-2008; Jakobsson,
Martin/F-6214-2010; Hindmarsh, Richard/C-1405-2012; Roche, Didier
M./C-9875-2010; Stroeven, Arjen/I-7330-2013; Hughes, Anna/J-5628-2015
OI Stroeven, Arjen/0000-0001-8812-2253; Stokes, Chris/0000-0003-3355-1573;
Livingstone, Stephen/0000-0002-7240-5037; Murton,
Julian/0000-0002-9469-5856; Hindmarsh, Richard/0000-0003-1633-2416;
Roche, Didier M./0000-0001-6272-9428; Margold,
Martin/0000-0001-5834-850X; Jakobsson, Martin/0000-0002-9033-3559;
Hughes, Anna/0000-0001-8584-5202
FU INQUA
FX This paper results from an INQUA (International Union for Quaternary
Research) project: 'Meltwater routing and Ocean-Cryosphere-Atmosphere
response (MOCA)'. We wish to thank INQUA for their generous financial
support and all those who participated in various MOCA workshops. We
also thank numerous colleagues who commented on sections of the
manuscript prior to submission, and the invaluable comments of two
anonymous referees. We are also grateful to Christine Batchelor and Nick
Golledge who provided Figure's 7 and 15, respectively. Any use of trade,
firm, or product names is for descriptive purposes only and does not
imply endorsement by the U.S. Government.
NR 396
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U2 61
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0277-3791
J9 QUATERNARY SCI REV
JI Quat. Sci. Rev.
PD OCT 1
PY 2015
VL 125
BP 15
EP 49
DI 10.1016/j.quascirev.2015.07.016
PG 35
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA CS4MH
UT WOS:000362049400002
ER
PT J
AU Jones, MR
Singels, A
Ruane, AC
AF Jones, M. R.
Singels, A.
Ruane, A. C.
TI Simulated impacts of climate change on water use and yield of irrigated
sugarcane in South Africa
SO AGRICULTURAL SYSTEMS
LA English
DT Article
DE Climate change; Model; Cane yield; Irrigation requirement; Water use
ID COUPLED MODEL; TEMPERATURE; GROWTH; CO2; PHOTOSYNTHESIS; ACCUMULATION;
PERFORMANCE; METABOLISM; BIOMASS
AB Reliable predictions of climate change impacts on water use, irrigation requirements and yields of irrigated sugarcane in South Africa (a water-scarce country) are necessary to plan adaptation strategies. Although previous work has been done in this regard, methodologies and results vary considerably. The objectives were (1) to estimate likely impacts of climate change on sugarcane yields, water use and irrigation demand at three irrigated sugarcane production sites in South Africa (Malelane, Pongola and La Mercy) for current (1980-2010) and future (2070-2100) climate scenarios, using an approach based on the Agricultural Model Intercomparison and Improvement Project (AgMIP) protocols; and (2) to assess the suitability of this methodology for investigating climate change impacts on sugarcane production.
Future climate datasets were generated using the Delta downscaling method and three Global Circulation Models (GCMs) assuming atmospheric CO2 concentration [CO2] of 734 ppm (A2 emissions scenario). Yield and water use were simulated using the DSSAT-Canegro v4.5 model.
Irrigated cane yields are expected to increase at all three sites (between 11 and 14%), primarily due to increased interception of radiation as a result of accelerated canopy development. Evapotranspiration and irrigation requirements increased by 11% due to increased canopy cover and evaporative demand. Sucrose yields are expected to decline because of increased consumption of photo-assimilate for structural growth and maintenance respiration. Crop responses in canopy development and yield formation differed markedly between the crop cycles investigated.
Possible agronomic implications of these results include reduced weed control costs due to shortened periods of partial canopy, a need for improved efficiency of irrigation to counter increased demands, and adjustments to ripening and harvest practices to counter decreased cane quality and optimise productivity. Although the Delta climate data downscaling method is considered robust, accurate and easily-understood, it does not change the future number of rain-days per month. The impacts of this and other climate data simplifications ought to be explored in future work. Shortcomings of the DSSAT-Canegro model include the simulated responses of phenological development, photosynthesis and respiration processes to high temperatures, and the disconnect between simulated biomass accumulation and expansive growth. Proposed methodology refinements should improve the reliability of predicted climate change impacts on sugarcane yield. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Jones, M. R.; Singels, A.] South African Sugarcane Res Inst, ZA-4300 Mt Edgecombe, South Africa.
[Singels, A.] Univ Pretoria, Dept Plant Prod & Soil Sci, ZA-0002 Pretoria, South Africa.
[Ruane, A. C.] NASA, Goddard Inst Space Studies, Climate Impacts Grp, New York, NY 10025 USA.
RP Jones, MR (reprint author), South African Sugarcane Res Inst, Private Bag X02, ZA-4300 Mt Edgecombe, South Africa.
EM matthew.jones@sugar.org.za; abraham.singels@sugar.org.za;
alexander.c.ruane@nasa.gov
OI Jones, Matthew/0000-0002-7703-4941; Singels, Abraham/0000-0003-4558-3003
FU South African Sugarcane Research Institute (SASRI)
FX This study was funded by the South African Sugarcane Research Institute
(SASRI). Many thanks to Phillemon Sithole and Shenay Harisunker at SASRI
for their assistance in preparing baseline weather datasets, and to the
AgMIP community for developing the methodologies used.
NR 52
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U1 6
U2 47
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0308-521X
EI 1873-2267
J9 AGR SYST
JI Agric. Syst.
PD OCT
PY 2015
VL 139
BP 260
EP 270
DI 10.1016/j.agsy.2015.07.007
PG 11
WC Agriculture, Multidisciplinary
SC Agriculture
GA CS0VE
UT WOS:000361779500022
ER
PT J
AU Mukherjee, M
Eikema, DJA
Chien, JH
Myers, SA
Scott-Pandorf, M
Bloomberg, JJ
Stergiou, N
AF Mukherjee, Mukul
Eikema, Diderik Jan A.
Chien, Jung Hung
Myers, Sara A.
Scott-Pandorf, Melissa
Bloomberg, Jacob J.
Stergiou, Nicholas
TI Plantar tactile perturbations enhance transfer of split-belt locomotor
adaptation
SO EXPERIMENTAL BRAIN RESEARCH
LA English
DT Article
DE Motor learning; Biomechanics; Touch; Vibration; Gait; Sensation;
Perception
ID PRESSURE DISTRIBUTION; HUMAN WALKING; SPACEFLIGHT; TREADMILL;
COORDINATION; MODULATION; SENSATION; REFLEXES; MUSCLES; BALANCE
AB Patterns of human locomotion are highly adaptive and flexible and depend on the environmental context. Locomotor adaptation requires the use of multisensory information to perceive altered environmental dynamics and generate an appropriate movement pattern. In this study, we investigated the use of multisensory information during locomotor learning. Proprioceptive perturbations were induced by vibrating tactors, placed bilaterally over the plantar surfaces. Under these altered sensory conditions, participants were asked to perform a split-belt locomotor task representative of motor learning. Twenty healthy young participants were separated into two groups: no-tactors (NT) and tactors (TC). All participants performed an overground walking trial, followed by treadmill walking including 18 min of split-belt adaptation and an overground trial to determine transfer effects. Interlimb coordination was quantified by symmetry indices and analyzed using mixed repeated-measures ANOVAs. Both groups adapted to the locomotor task, indicated by significant reductions in gait symmetry during the split-belt task. No significant group differences in spatiotemporal and kinetic parameters were observed on the treadmill. However, significant group differences were observed overground. Step and swing time asymmetries learned on the split-belt treadmill were retained and decayed more slowly overground in the TC group whereas in NT, asymmetries were rapidly lost. These results suggest that tactile stimulation contributed to increased lower limb proprioceptive gain. High proprioceptive gain allows for more persistent overground after effects, at the cost of reduced adaptability. Such persistence may be utilized in populations displaying pathologic asymmetric gait by retraining a more symmetric pattern.
C1 [Mukherjee, Mukul; Eikema, Diderik Jan A.; Chien, Jung Hung; Myers, Sara A.; Stergiou, Nicholas] Univ Nebraska, Sch Hlth Phys Educ & Recreat, Omaha, NE 68182 USA.
[Scott-Pandorf, Melissa] NASA Johnson Space Ctr, Wyle Sci Technol & Engn, Houston, TX USA.
[Bloomberg, Jacob J.] NASA Johnson Space Ctr, Neurosci Labs, Houston, TX USA.
[Stergiou, Nicholas] Univ Nebraska, Med Ctr, Coll Publ Hlth, Dept Environm Agr & Occupat Hlth, Omaha, NE 68182 USA.
RP Mukherjee, M (reprint author), Univ Nebraska, Sch Hlth Phys Educ & Recreat, Biomech Res Bldg, Omaha, NE 68182 USA.
EM mmukherjee@unomaha.edu
OI Mukherjee, Mukul/0000-0001-9653-0556
FU NASA Experimental Program to Stimulate Competitive Research (EPSCoR)
[NNX11AM06A]; National Institute of General Medical Sciences of the
National Institutes of Health [P20GM109090]; Rehabilitation Research and
Development Service of the VA Office of Research and Development
[1I01RX000604]
FX This study was supported by funds from the NASA Experimental Program to
Stimulate Competitive Research (EPSCoR) award number NNX11AM06A, the
National Institute of General Medical Sciences of the National
Institutes of Health award number P20GM109090 and award number
1I01RX000604 from the Rehabilitation Research and Development Service of
the VA Office of Research and Development. The content is solely the
responsibility of the authors and does not necessarily represent the
official views of the NASA, NIH or the VA Office of Research and
Development.
NR 26
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U1 1
U2 5
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0014-4819
EI 1432-1106
J9 EXP BRAIN RES
JI Exp. Brain Res.
PD OCT
PY 2015
VL 233
IS 10
BP 3005
EP 3012
DI 10.1007/s00221-015-4370-1
PG 8
WC Neurosciences
SC Neurosciences & Neurology
GA CR8WU
UT WOS:000361635800022
PM 26169104
ER
PT J
AU Edwards, CS
Ehlmann, BL
AF Edwards, Christopher S.
Ehlmann, Bethany L.
TI Carbon sequestration on Mars
SO GEOLOGY
LA English
DT Article
ID IDENTIFICATION; ENVIRONMENTS; CLIMATE; CRATER; ROCKS
AB On Earth, carbon sequestration in geologic units plays an important role in the carbon cycle, scrubbing CO2 from the atmosphere for long-term storage. While carbonate is identified in low abundances within the dust and soils of Mars, at < 1 wt% in select meteorites, and in limited outcrops, no massive carbonate rock reservoir on Mars has been identified to date. Here, we investigate the largest exposed carbonate-bearing rock unit, the Nili Fossae plains, combining spectral, thermophysical, and morphological analyses to evaluate the timing and carbon sequestration potential of rocks on Mars. We find that the olivine-enriched (similar to 20%-25%) basalts have been altered, by low-temperature in situ carbonation processes, to at most similar to 20% Fe-Mg carbonate, thus limiting carbon sequestration in the Nili Fossae region to similar to 0.25-12 mbar of CO2 during the late Noachian-early Hesperian, before or concurrent with valley network formation. While this is large compared to modern-day CO2 reservoirs, the lack of additional, comparably sized post-late Noachian carbonate-bearing deposits on Mars indicates ineffective carbon sequestration in rock units over the past similar to 3.7 b.y. This implies a thin atmosphere (less than or similar to 500 mbar) during valley network formation, extensive post-Noachian atmospheric loss to space, or diffuse, deep sequestration by a yet-to-be understood process. In stark contrast to Earth's biologically mediated crust: atmosphere carbon reservoir ratio of similar to 10(4)-10(5), Mars' ratio is a mere similar to 10-10(3), even if buried pre-Noachian crust holds multiple bars.
C1 [Edwards, Christopher S.; Ehlmann, Bethany L.] CALTECH, Pasadena, CA 91125 USA.
[Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Edwards, CS (reprint author), US Geol Survey, Astrogeol Sci Ctr, 2255 N Gemini Rd, Flagstaff, AZ 86001 USA.
FU Jet Propulsion Laboratory
FX We thank R.E. Arvidson for providing the CRISM DISORT processed image,
A.D. Rogers for the Syrtis-type TES spectra, and S. Piqueux for helpful
discussions. T.D. Glotch, P.D. Niles, and an anonymous reviewer provided
helpful formal reviews. A Mars Exploration Program Future Landing Sites
grant administered by the Jet Propulsion Laboratory provided partial
support for Edwards and Ehlmann to conduct this analysis.
NR 31
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U1 8
U2 33
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
EI 1943-2682
J9 GEOLOGY
JI Geology
PD OCT
PY 2015
VL 43
IS 10
BP 863
EP 866
DI 10.1130/G36983.1
PG 4
WC Geology
SC Geology
GA CS1MQ
UT WOS:000361830400004
ER
PT J
AU Daly, AM
Drouin, BJ
Pearson, JC
Sung, K
Brown, LR
Mantz, A
Smith, MAH
AF Daly, Adam M.
Drouin, Brian J.
Pearson, John C.
Sung, Keeyoon
Brown, Linda R.
Mantz, Arlan
Smith, Mary Ann H.
TI The v(17) band of C2H5D from 770 to 880 cm(-1)
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE d1-Ethane; Infrared spectroscopy; High resolution; Line intensities;
FT-IR
ID TORSIONAL RAMAN-SPECTRA; DEUTERATED ETHANES; SPECTROSCOPY; COEFFICIENTS;
INTENSITIES; ATMOSPHERE; RESOLUTION; MOLECULES; ENERGIES; CH3CH2D
AB Atmospheric investigations rely heavily on the availability of accurate spectral information of hydrocarbons. To extend the ethane database we recorded a 0.0028 cm(-1) resolution spectrum of (C2H5D)-C-12 from 650 to 1500 cm(-1) using a Bruker Fourier Transform spectrometer IFS-125HR at the Jet Propulsion Laboratory. The 98% deuterium-enriched sample was contained in a 0.2038 m absorption cell; one spectrum was obtained with the sample cryogenically cooled to 130.5 K and another at room temperature. From the cold data, we retrieved line positions and intensities of 8704 individual absorption features from 770 to 880 cm(-1) using a least squares curve fitting algorithm. From this set of measurements, we assigned 5035 transitions to the v(17) fundamental at 805.342729(27) cm(-1); this band is a c-type vibration, with often-resolved A and E components arising from internal rotation. The positions were modeled to a 22 term torsional Hamiltonian using SPFIT to fit the spectrum to a standard deviation of 7 x 10(-4) cm(-1) (21 MHz). The prediction of the 5035 line intensities at 130.5 K agreed with observed intensities, but a small centrifugal distortion type correction to the transition dipole was needed to model the intensity of high K-a R and P transitions. The integrated band intensities of 3.6628 x 10(-19) cm(-1)/(molecule cm(-2)) at 296 K in the 770-880 cm(-1) region was obtained. To predict line intensities at different temperatures, the partition function values were determined at nine temperatures between 9.8 and 300 K by summing individual energy levels up to J = 99 and K-a = 99 for the six states up through v(17) at 805 cm(-1). We found the energy of A and E are inverted as compared to ground state (with the E state lower than the A state) and the splitting, -241.8(10) MHz, lies between the ground state value of +74.167(18) MHz and the first torsional state (v(18) = 271.1 cm(-1)) value of -3382.23(34) MHz. The proximity of the energy splitting to the ground state suggests that the v(17) state has a similar torsional character. The resulting prediction of singly-deuterated ethane absorption at 12.51 mu m enables its detection in planetary atmospheres, including those of Titan and exoplanets. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Daly, Adam M.; Drouin, Brian J.; Pearson, John C.; Sung, Keeyoon; Brown, Linda R.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA.
[Mantz, Arlan] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA.
[Smith, Mary Ann H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
RP Brown, LR (reprint author), CALTECH, Jet Prop Lab, Mailstop 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM adaly@email.arizona.edu; Linda.R.Brown@jpl.nasa.gov
RI Sung, Keeyoon/I-6533-2015
FU NASA Langley Research Center; National Aeronautics and Space
Administration
FX The research described in this paper was performed at the Jet Propulsion
Laboratory, California Institute of Technology, Connecticut College, and
NASA Langley Research Center under contracts and grants with the
National Aeronautics and Space Administration. We thank Dr. Steve Vance
at JPL for sharing his ethane-D1 gas sample. The authors would like to
thank Peter Groner for several rounds of conversations regarding the
analysis of C2H5D.
NR 30
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U1 1
U2 9
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD OCT
PY 2015
VL 316
BP 1
EP 10
DI 10.1016/j.jms.2015.06.006
PG 10
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA CR8ZY
UT WOS:000361644200001
ER
PT J
AU Arcadias, L
Corbet, R
AF Arcadias, Laurence
Corbet, Robin
TI ANIMATING FERMI-A COLLABORATION BETWEEN ART STUDENTS AND ASTRONOMERS
SO LEONARDO
LA English
DT Editorial Material
ID SPACE
AB Undergraduate animation students at the Maryland Institute College of Art teamed up with scientists from the Fermi Gamma-ray Space Telescope to produce a set of animations on several astronomy topics. Here, the authors describe the process and discuss the results, educational benefits and the cross-cultural experience. These animations are available for free online.
C1 [Arcadias, Laurence] Maryland Inst Coll Art, Animat Dept, Baltimore, MD 21217 USA.
[Corbet, Robin] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
[Corbet, Robin] NASA, Goddard Space Flight Ctr, Astrophys Lab, Greenbelt, MD 20771 USA.
RP Arcadias, L (reprint author), Maryland Inst Coll Art, Animat Dept, Baltimore, MD 21217 USA.
EM larcadias@mica.edu; corbet@umbc.edu
NR 10
TC 0
Z9 0
U1 1
U2 3
PU MIT PRESS
PI CAMBRIDGE
PA ONE ROGERS ST, CAMBRIDGE, MA 02142-1209 USA
SN 0024-094X
EI 1530-9282
J9 LEONARDO
JI Leonardo
PD OCT
PY 2015
VL 48
IS 5
BP 484
EP 485
DI 10.1162/LEON_a_01123
PG 2
WC Art
SC Art
GA CS1QG
UT WOS:000361841800016
ER
PT J
AU Tian, ZH
Yu, LY
Leckey, C
Seebo, J
AF Tian, Zhenhua
Yu, Lingyu
Leckey, Cara
Seebo, Jeffrey
TI Guided wave imaging for detection and evaluation of impact-induced
delamination in composites
SO SMART MATERIALS AND STRUCTURES
LA English
DT Article
DE guided waves; frequency wavenumber analysis; delamination
quantification; laser vibrometry sensing
ID LAMB WAVES; NUMBER ANALYSIS; DAMAGE; INTEGRATION
AB In this paper, guided wavefield interactions with delamination damage in laminated composite panels are investigated. The frequency-wavenumber representations of the guided wavefields show that different wavenumbers are present in the delaminated plate, compared to a pristine case. The wavenumbers are correlated to trapped waves in the delamination region. Novel approaches for imaging the composite panels using guided waves are discussed and demonstrated for quantitative evaluation of the delamination damage. A filter reconstruction imaging method is shown to provide a rapid technique to locate delamination damage by showing where guided wave energy is trapped. A spatial wavenumber-based imaging algorithm is applied to calculate wavenumber values at each spatial location and highlights the delamination damage as regions with larger wavenumber values. The imaging approaches are demonstrated using experimental data from a plate with a simulated delamination (teflon insert) and from a plate containing impact-induced delamination damage. The methods are also applied to a multiple mode guided wave case to demonstrate application to complex wave cases.
C1 [Tian, Zhenhua; Yu, Lingyu] Univ S Carolina, Dept Mech Engn, Columbia, SC 29208 USA.
[Leckey, Cara] NASA Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23681 USA.
[Seebo, Jeffrey] Analyt Mech Associates Inc, Hampton, VA 23681 USA.
RP Tian, ZH (reprint author), Univ S Carolina, Dept Mech Engn, Columbia, SC 29208 USA.
EM tianz@email.sc.edu
FU SC NASA EPSCoR Research and Education Awards Program (REAP)
[21-NE-USC_Yu-RGP]
FX The authors would like to thank (1) the non-reimbursement space act
umbrella agreement SAA1-1181 between South Carolina Research Foundation
(SCRF) and the National Aeronautics and Space Administration (NASA)
Langley Research Center, (2) University of South Carolina SPARC graduate
fellowship, and (3) SC NASA EPSCoR Research and Education Awards Program
(REAP) 21-NE-USC_Yu-RGP.
NR 50
TC 3
Z9 3
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0964-1726
EI 1361-665X
J9 SMART MATER STRUCT
JI Smart Mater. Struct.
PD OCT
PY 2015
VL 24
IS 10
AR 105019
DI 10.1088/0964-1726/24/10/105019
PG 13
WC Instruments & Instrumentation; Materials Science, Multidisciplinary
SC Instruments & Instrumentation; Materials Science
GA CS1OT
UT WOS:000361836800019
ER
PT J
AU Della Corte, C
AF Della Corte, Christopher
TI Tribology's Origin
SO TRIBOLOGY & LUBRICATION TECHNOLOGY
LA English
DT Letter
C1 NASA, Glenn Res Ctr, Tribol & Rotating Machinery, Cleveland, OH 44135 USA.
RP Della Corte, C (reprint author), NASA, Glenn Res Ctr, Tribol & Rotating Machinery, Cleveland, OH 44135 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS
PI PARK RIDGE
PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA
SN 1545-858X
J9 TRIBOL LUBR TECHNOL
JI Tribol. Lubr. Technol.
PD OCT
PY 2015
VL 71
IS 10
BP 7
EP 7
PG 1
WC Engineering, Mechanical
SC Engineering
GA CS1VD
UT WOS:000361855700003
ER
PT J
AU Follette-Cook, MB
Pickering, KE
Crawford, JH
Duncan, BN
Loughner, CP
Diskin, GS
Fried, A
Weinheimer, AJ
AF Follette-Cook, Melanie B.
Pickering, Kenneth E.
Crawford, James H.
Duncan, Bryan N.
Loughner, Christopher P.
Diskin, Glenn S.
Fried, Alan
Weinheimer, Andrew J.
TI Spatial and temporal variability of trace gas columns derived from
WRF/Chem regional model output: Planning for geostationary observations
of atmospheric composition
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Geostationary; Air quality; DISCOVER-AQ; TEMPO; Variability; WRF/Chem
ID ABSORPTION SPECTROMETER GEOSCIA; EXPLORER GEOTROPE MISSION; TROPOSPHERIC
POLLUTION; UNITED-STATES; REQUIREMENTS; EMISSIONS; OZONE; SPACE;
CAPABILITIES; CHEMISTRY
AB We quantify both the spatial and temporal variability of column integrated O-3, NO2, CO, SO2, and HCHO over the Baltimore/Washington, DC area using output from the Weather Research and Forecasting model with on-line chemistry (WRF/Chem) for the entire month of July 2011, coinciding with the first deployment of the NASA Earth Venture program mission Deriving Information on Surface conditions from Column and Vertically Resolved Observations Relevant to Air Quality (DISCOVER-AQ). Using structure function analyses, we find that the model reproduces the spatial variability observed during the campaign reasonably well, especially for O-3. The Tropospheric Emissions: Monitoring of Pollution (TEMPO) instrument will be the first NASA mission to make atmospheric composition observations from geostationary orbit and partially fulfills the goals of the Geostationary Coastal and Air Pollution Events (GEO-CAPE) mission. We relate the simulated variability to the precision requirements defined by the science traceability matrices of these space-borne missions. Results for O-3 from 0 to 2 km altitude indicate that the TEMPO instrument would be able to observe O-3 air quality events over the Mid-Atlantic area, even on days when the violations of the air quality standard are not widespread. The results further indicated that horizontal gradients in CO from 0 to 2 km would be observable over moderate distances (>20 km). The spatial and temporal results for tropospheric column NO2 indicate that TEMPO would be able to observe not only the large urban plumes at times of peak production, but also the weaker gradients between rush hours. This suggests that the proposed spatial and temporal resolutions for these satellites as well as their prospective precision requirements are sufficient to answer the science questions they are tasked to address. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Follette-Cook, Melanie B.] Morgan State Univ, GESTAR, Baltimore, MD 21251 USA.
[Follette-Cook, Melanie B.; Pickering, Kenneth E.; Duncan, Bryan N.; Loughner, Christopher P.] NASA, Goddard Space Flight Ctr, New York, NY USA.
[Crawford, James H.; Diskin, Glenn S.] NASA, Langley Res Ctr, New York, NY USA.
[Loughner, Christopher P.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, Baltimore, MD USA.
[Fried, Alan] Univ Colorado, Boulder, CO 80309 USA.
[Weinheimer, Andrew J.] Natl Ctr Atmospher Res, New York, NY USA.
RP Follette-Cook, MB (reprint author), Morgan State Univ, GESTAR, Baltimore, MD 21251 USA.
EM Melanie.cook@nasa.gov
RI Pickering, Kenneth/E-6274-2012; Duncan, Bryan/A-5962-2011;
OI Loughner, Christopher/0000-0002-3833-2014
FU NASA Earth Venture-1 DISCOVER-AQ project; GEO-CAPE Atmospheric Science
Working Group
FX This work was supported under the NASA Earth Venture-1 DISCOVER-AQ
project and the GEO-CAPE Atmospheric Science Working Group.
Contributions from Chinmay Satam for the processing of emissions data
are gratefully acknowledged. We also thank Dr. Jack Fishman for his
valuable input.
NR 31
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U1 4
U2 28
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 OCT
PY 2015
VL 118
BP 28
EP 44
DI 10.1016/j.atmosenv.2015.07.024
PG 17
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CR5UM
UT WOS:000361409900004
ER
PT J
AU Kharol, SK
Martin, RV
Philip, S
Boys, B
Lamsal, LN
Jerrett, M
Brauer, M
Crouse, DL
McLinden, C
Burnett, RT
AF Kharol, S. K.
Martin, R. V.
Philip, S.
Boys, B.
Lamsal, L. N.
Jerrett, M.
Brauer, M.
Crouse, D. L.
McLinden, C.
Burnett, R. T.
TI Assessment of the magnitude and recent trends in satellite-derived
ground-level nitrogen dioxide over North America
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE OMI; NO2; GEOS-Chem; Trend; North America
ID LAND-USE REGRESSION; OZONE MONITORING INSTRUMENT; FINE PARTICULATE
MATTER; AMBIENT AIR-POLLUTION; IN-SITU MEASUREMENTS; UNITED-STATES;
SURFACE MEASUREMENTS; EXPOSURE ASSESSMENT; NO2 CONCENTRATIONS;
TROPOSPHERIC NO2
AB We estimate ground-level nitrogen dioxide (NO2) concentrations from the OMI (Ozone Monitoring Instrument) over North America for the period 2005-2012. A chemical transport model (GEOS-Chem) is used to account for effects of the NO2 profile on the column retrieval, and to relate OMI NO2 columns to ground-level concentrations. The magnitude of the period-mean OMI-derived NO2 concentrations is evaluated versus in situ measurements from air quality networks yielding a significant spatial correlation (r = 0.81) but OMI-derived values are lower with a slope of 0.4. Comparison of the in situ concentrations versus spatially resolved concentrations estimated from land use regression models reveals that this difference partially arises from representativeness difference due to preferential placement of in situ monitors at locations with enhanced NO2, coupled with the OMI horizontal resolution. In situ observations provide information about local concentrations while OMI offers area-averaged information. The remaining difference is less readily explained and appears to include a combination of the effects of local unresolved geophysical processes affecting both the NO2 retrieval and the vertical profile used to relate the column to ground level. We also evaluate trends over North America from OMI and in situ measurements for the period of 2005-2012. OMI derived ground-level NO2 well reproduces the spatial pattern of the in situ trends (r = 0.77) and the slope of 0.4 versus the trend from in situ monitors is consistent with the slope versus mean concentrations. Absolute regional trends inferred from in situ measurements alone may overestimate area average changes. Nonetheless coincidently sampled ground-level NO2 concentrations from OMI and in situ measurements for 2005-2012 exhibit similar relative decreases over Eastern (-6.5 +/- 2.0%/yr, -7.1 +/- 1.3%/yr), Western (-4.5 +/- 1.1%/yr, -6.5 +/- 0.7%/yr) and Central (-3.3 +/- 2.3%/yr, -4.1 +/- 0.8%/yr) North America. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Kharol, S. K.; Martin, R. V.; Philip, S.; Boys, B.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Kharol, S. K.; McLinden, C.] Environm Canada, Air Qual Res Div, Toronto, ON, Canada.
[Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lamsal, L. N.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA.
[Lamsal, L. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jerrett, M.] Univ Calif Berkeley, Sch Publ Hlth, Div Environm Hlth Sci, Berkeley, CA 94720 USA.
[Brauer, M.] Univ British Columbia, Sch Populat & Publ Hlth, Vancouver, BC V5Z 1M9, Canada.
[Crouse, D. L.; Burnett, R. T.] Hlth Canada, Populat Studies Div, Ottawa, ON K1A 0L2, Canada.
RP Kharol, SK (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
EM shaileshan2000@gmail.com
RI Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014
OI Martin, Randall/0000-0003-2632-8402;
FU Environment Canada [1113957]; Health Canada [4500275460]; Collaborative
Health Research Project of the Natural Sciences and Engineering Research
Council of Canada [398578 - 11]; Canadian Institutes of Health Research
FX The authors acknowledge National Aeronautics and Space Administration
(NASA) for the free use of NO2 tropospheric column data from
the OMI sensor. This work was funded by Environment Canada (1113957),
Health Canada (4500275460) and a Collaborative Health Research Project
(398578 - 11) of the Natural Sciences and Engineering Research Council
of Canada, and the Canadian Institutes of Health Research.
NR 70
TC 5
Z9 5
U1 1
U2 16
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 OCT
PY 2015
VL 118
BP 236
EP 245
DI 10.1016/j.atmosenv.2015.08.011
PG 10
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CR5UM
UT WOS:000361409900024
ER
PT J
AU Desaraju, VR
Michael, N
Humenberger, M
Brockers, R
Weiss, S
Nash, J
Matthies, L
AF Desaraju, Vishnu R.
Michael, Nathan
Humenberger, Martin
Brockers, Roland
Weiss, Stephan
Nash, Jeremy
Matthies, Larry
TI Vision-based landing site evaluation and informed optimal trajectory
generation toward autonomous rooftop landing
SO AUTONOMOUS ROBOTS
LA English
DT Article; Proceedings Paper
CT 10th Conference on Robotics - Science and Systems (RSS)
CY JUN, 2014
CL Univ Calif, Berkeley, CA
HO Univ Calif
ID MONOCULAR VISION; HELICOPTER; TERRAIN; TARGET
AB Autonomous landing is an essential function for micro air vehicles (MAVs) for many scenarios. We pursue an active perception strategy that enables MAVs with limited onboard sensing and processing capabilities to concurrently assess feasible rooftop landing sites with a vision-based perception system while generating trajectories that balance continued landing site assessment and the requirement to provide visual monitoring of an interest point. The contributions of the work are twofold: (1) a perception system that employs a dense motion stereo approach that determines the 3D model of the captured scene without the need of geo-referenced images, scene geometry constraints, or external navigation aids; and (2) an online trajectory generation approach that balances the need to concurrently explore available rooftop vantages of an interest point while ensuring confidence in the landing site suitability by considering the impact of landing site uncertainty as assessed by the perception system. Simulation and experimental evaluation of the performance of the perception and trajectory generation methodologies are analyzed independently and jointly in order to establish the efficacy and robustness of the proposed approach.
C1 [Desaraju, Vishnu R.; Michael, Nathan] Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA.
[Brockers, Roland; Weiss, Stephan; Nash, Jeremy; Matthies, Larry] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Humenberger, Martin] AIT, Vienna, Austria.
RP Desaraju, VR (reprint author), Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA.
EM rajeswar@cmu.edu; nmichael@cmu.edu; martin.humenberger@ait.ac.at;
roland.brockers@jpl.nasa.gov; stephan.m.weiss@jpl.nasa.gov;
jeremy.nash@jpl.nasa.gov; lhm@jpl.nasa.gov
FU ARL [W911NF-08-2-0004]
FX We gratefully acknowledge the support of ARL Grant W911NF-08-2-0004.
NR 44
TC 0
Z9 0
U1 2
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0929-5593
EI 1573-7527
J9 AUTON ROBOT
JI Auton. Robot.
PD OCT
PY 2015
VL 39
IS 3
SI SI
BP 445
EP 463
DI 10.1007/s10514-015-9456-x
PG 19
WC Computer Science, Artificial Intelligence; Robotics
SC Computer Science; Robotics
GA CR6LV
UT WOS:000361459500014
ER
PT J
AU Hoffmayer, ER
Hendon, JM
Parsons, GR
Driggers, WB
Campbell, MD
AF Hoffmayer, Eric R.
Hendon, Jill M.
Parsons, Glenn R.
Driggers, William B., III
Campbell, Matthew D.
TI A comparison of single and multiple stressor protocols to assess acute
stress in a coastal shark species, Rhizoprionodon terraenovae
SO FISH PHYSIOLOGY AND BIOCHEMISTRY
LA English
DT Article
DE Carcharhinidae; Glucose; Lactate; Osmolality; Hematocrit; Stress
response
ID ATLANTIC SHARPNOSE SHARK; JUVENILE CHINOOK SALMON; GILL-NET CAPTURE;
PHYSIOLOGICAL-RESPONSE; ACID-BASE; HANDLING STRESS; ION BALANCE; FISH;
ELASMOBRANCH; MORTALITY
AB Elasmobranch stress responses are traditionally measured in the field by either singly or serially sampling an animal after a physiologically stressful event. Although capture and handling techniques are effective at inducing a stress response, differences in protocols could affect the degree of stress experienced by an individual, making meaningful comparisons between the protocols difficult, if not impossible. This study acutely stressed Atlantic sharpnose sharks, Rhizoprionodon terraenovae, by standardized capture (rod and reel) and handling methods and implemented either a single or serial blood sampling protocol to monitor four indicators of the secondary stress response. Single-sampled sharks were hooked and allowed to swim around the boat until retrieved for a blood sample at either 0, 15, 30, 45, or 60 min post-hooking. Serially sampled sharks were retrieved, phlebotomized, released while still hooked, and subsequently resampled at 15, 30, 45, and 60 min intervals post-hooking. Blood was analyzed for hematocrit, and plasma glucose, lactate, and osmolality levels. Although both single and serial sampling protocols resulted in an increase in glucose, no significant difference in glucose level was found between protocols. Serially sampled sharks exhibited cumulatively heightened levels for lactate and osmolality at all time intervals when compared to single-sampled animals at the same time. Maximal concentration differences of 217.5, 9.8, and 41.6 % were reported for lactate, osmolality, and glucose levels, respectively. Hematocrit increased significantly over time for the single sampling protocol but did not change significantly during the serial sampling protocol. The differences in resultant blood chemistry levels between implemented stress protocols and durations are significant and need to be considered when assessing stress in elasmobranchs.
C1 [Hoffmayer, Eric R.; Parsons, Glenn R.] Univ Mississippi, Dept Biol, University, MS 38677 USA.
[Hoffmayer, Eric R.; Driggers, William B., III; Campbell, Matthew D.] Mississippi Labs, Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Pascagoula, MS 39567 USA.
[Hendon, Jill M.] Univ So Mississippi, Ctr Fisheries Res & Dev, Gulf Coast Res Lab, Ocean Springs, MS 39564 USA.
RP Hoffmayer, ER (reprint author), Mississippi Labs, Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, 3209 Frederic St, Pascagoula, MS 39567 USA.
EM eric.hoffmayer@noaa.gov
FU National Marine Fisheries Service (MARFIN) [NA77FF0548]
FX Financial support for this project was partially provided by the
National Marine Fisheries Service (MARFIN # NA77FF0548) to G. Parsons.
Sampling protocols were approved by the University of Mississippi's
Institutional Animal Care and Use Committee (# 99-006). This project
would not have been possible without the help of many volunteers. We
would like to thank J. Bartlett, J. Horton, K. Larsen, G. Gray, R.
Hoffmayer, A. Lee, D. Drury, R. McCall, G. Zapfe, and W. Dempster for
their assistance in the field. We also thank M.S. Peterson, J.S. Franks,
and G. Pellegrin for their critical review and advice on this
manuscript.
NR 38
TC 2
Z9 2
U1 2
U2 25
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0920-1742
EI 1573-5168
J9 FISH PHYSIOL BIOCHEM
JI Fish Physiol. Biochem.
PD OCT
PY 2015
VL 41
IS 5
BP 1253
EP 1260
DI 10.1007/s10695-015-0083-4
PG 8
WC Biochemistry & Molecular Biology; Fisheries; Physiology
SC Biochemistry & Molecular Biology; Fisheries; Physiology
GA CR7OC
UT WOS:000361539100013
PM 26026297
ER
PT J
AU Frigeri, A
De Sanctis, MC
Ammannito, E
Tosi, F
Longobardo, A
Zambon, F
McCord, T
Combe, JP
Jaumann, R
Raymond, CA
Russell, CT
AF Frigeri, A.
De Sanctis, M. C.
Ammannito, E.
Tosi, F.
Longobardo, A.
Zambon, F.
McCord, T.
Combe, J. P.
Jaumann, R.
Raymond, C. A.
Russell, C. T.
TI The spectral parameter maps of Vesta from VIR data
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Spectroscopy; Mineralogy; Geological processes
ID FRAMING CAMERA IMAGES; REFLECTANCE SPECTROSCOPY; SOLAR-SYSTEM; DAWN;
SPECTROMETER; DIVERSITY; PYROXENES; MISSION; MARS
AB Here we present the spectral parameter maps used in this Surface Composition of Vesta Special Issue. The use of spectral parameters have been important since the first ground-based observations of Vesta as they can describe single mineralogic aspects as abundances or change in surface composition. Mapping these parameters over the surface shows the mineralogic diversity across the asteroid Vesta. In this work we discuss the development of the maps, which are produced from the data of the Visible and Infrared mapping spectrometer onboard NASA's Dawn mission. We describe how we processed the VIR spectra and how we produced the geometries of data acquisition. Spectra and geometries are used to design a Geographic Information System procedure to mosaic these data. We conclude the article with a description of the trends of the pyroxene-related spectral parameters across the asteroid, and some statistics on the spectral parameters of each map within the quadrangle-based scheme used in this special issue. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Frigeri, A.; De Sanctis, M. C.; Tosi, F.; Longobardo, A.; Zambon, F.] IAPS, Ist Nazl Astrofis INAF, I-00133 Rome, Italy.
[Jaumann, R.] Inst Planetary Res, German Aerosp Ctr, Berlin, Germany.
[McCord, T.; Combe, J. P.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ammannito, E.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
RP Frigeri, A (reprint author), IAPS, Ist Nazl Astrofis INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
EM alessandro.frigeri@iaps.inaf.it
RI Frigeri, Alessandro/F-2151-2010;
OI Frigeri, Alessandro/0000-0002-9140-3977; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Tosi, Federico/0000-0003-4002-2434;
Zambon, Francesca/0000-0002-4190-6592
FU ASI; NASA; Italian Space Agency ASI; Dawn Science, Instrument,
Operations and current and future working teams
FX This work was supported by ASI and NASA. VIR is funded by the Italian
Space Agency ASI and was developed under the leadership of INAF-Istituto
di Astrofisica e Planetologia Spaziali, Rome, Italy. The instrument was
built by Selex-Galileo, Florence, Italy. The authors are grateful the
support of the Dawn Science, Instrument, Operations and current and
future working teams.
NR 31
TC 9
Z9 9
U1 1
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD OCT
PY 2015
VL 259
SI SI
BP 10
EP 20
DI 10.1016/j.icarus.2015.06.027
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR3UL
UT WOS:000361258500002
ER
PT J
AU Combe, JP
Ammannito, E
Tosi, F
De Sanctis, MC
McCord, TB
Raymond, CA
Russell, CT
AF Combe, Jean-Philippe
Ammannito, Eleonora
Tosi, Federico
De Sanctis, Maria Cristina
McCord, Thomas B.
Raymond, Carol A.
Russell, Christopher T.
TI Reflectance properties and hydrated material distribution on Vesta:
Global investigation of variations and their relationship using improved
calibration of Dawn VIR mapping spectrometer
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids, composition; Mineralogy; Spectroscopy
ID ASTEROID 4 VESTA; DARK MATERIAL; BIDIRECTIONAL REFLECTANCE;
THERMAL-PROPERTIES; FRAMING CAMERA; SURFACE; MINERALOGY; REGOLITH;
SPECTROSCOPY; SAMPLES
AB Vesta's surface albedo variations and hydrated material content share similar spatial distribution. This observation is consistent with carbonaceous chondrite meteorites as a likely source material for dark surface units observed by the Dawn spacecraft, as presented by numerous publications. While these deposits have been studied extensively by analysis of data from the Framing Camera (FC) and the Visible and Infrared Spectrometer (VIR), we performed a new analysis based on an improved calibration of VIR. First we identified instrument and calibration artifacts, and we therefore developed corrections of the VIR flat field and response function. Then we developed a photometric correction for Vesta based on the lunar model by Shkuratov et al. (Shkuratov, Yu.G. et al. [1999]. Icarus 141, 132-155. http://dx.doi.org/10.1006/icar.1999.6154), and a semi-analytical inversion of the photometric parameters. This photometric model combines minimization of the scattering effects due to the topography (a disk function) and variations of multiple-scattering with phase angle (the phase function) caused by microscopic physical properties of the regolith. The improved calibration and photometric correction enable more accurate analysis of the spectral properties of Vesta's surface material, especially the reflectance at 1.4 mu m and the 2.8 mu m hydroxyl absorption band depth. We produced global and quadrangle maps that are used as a common dataset for this Icarus special issue on Vesta's surface composition. The joint interpretation of both the 1.4 mu m reflectance and the 2.8 mu m absorption band depth reveals unusual spectral properties for a number of impact craters and ejecta compared to the rest of Vesta. An area including the Bellicia, Arruntia and Pomponia craters, where olivine might be present, has relatively high reflectance and a strong hydroxyl absorption band. Another area in the vicinity of Capparonia crater has a high content of hydrated materials, although with moderate reflectance and typical pyroxene-rich composition. Ejecta blankets west of Oppia crater have a spectral behavior similar to Capparonia, except for the wider and more complex shape of the hydroxyl absorption band. On the other hand, some low-hydrated areas associated to crater floors and ejecta have higher reflectance and steeper spectral slope than most low-hydrated terrains Vesta. A broad lane that extends from Rheasilvia rim at Matronalia Rupes to the northern regions hosts little to no hydrated materials and exhibits a moderate spectral slope, similar to Rheasilvia's basin floor. These properties reinforce the hypothesis that the lane is composed of ejecta from Rheasilvia, as indicated by the distribution of pyroxene compositions by previous results from Dawn. A few small and fresh craters exhibit an association between low-reflectance, little to no hydrated materials and a strong positive spectral slope, suggesting optical effects by opaque coatings, as opposed to carbonaceous chondrite deposits, and possible coarser grains. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Combe, Jean-Philippe; McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Ammannito, Eleonora; Tosi, Federico; De Sanctis, Maria Cristina] Ist Astrofis & Planetol Spaziali Ist Nazl Astrofi, I-00133 Rome, Italy.
[Ammannito, Eleonora; Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Raymond, Carol A.] Jet Prop Lab, Pasadena, CA 91109 USA.
RP Combe, JP (reprint author), Bear Fight Inst, 22 Fiddlers Rd,POB 667, Winthrop, WA 98862 USA.
EM jean-philippe_combe@bearfightinstitute.com
OI Tosi, Federico/0000-0003-4002-2434
FU NASA Dawn mission from University of California, Los Angeles
[2090-S-MB516]; ASI (Italian Space Agency); INAF (Istituto Nazionale di
Astrofisica)
FX The funding for this research was provided under the NASA Dawn mission
through a subcontract 2090-S-MB516 from the University of California,
Los Angeles. The VIR instrument and VIR team are funded by ASI (Italian
Space Agency) and INAF (Istituto Nazionale di Astrofisica).
NR 57
TC 7
Z9 7
U1 1
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD OCT
PY 2015
VL 259
SI SI
BP 21
EP 38
DI 10.1016/j.icarus.2015.07.034
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR3UL
UT WOS:000361258500003
ER
PT J
AU Prettyman, TH
Yamashita, N
Reedy, RC
McSween, HY
Mittlefehldt, DW
Hendricks, JS
Toplis, MJ
AF Prettyman, T. H.
Yamashita, N.
Reedy, R. C.
McSween, H. Y., Jr.
Mittlefehldt, D. W.
Hendricks, J. S.
Toplis, M. J.
TI Concentrations of potassium and thorium within Vesta's regolith
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids, composition; Gamma ray spectroscopy;
Planetary formation; Meteorites
ID MAGMA OCEAN CRYSTALLIZATION; DIOGENITE PARENT BODY; DAWNS GAMMA-RAY;
LUNAR-SURFACE; DARK MATERIAL; ELEMENTAL COMPOSITION; POLYMICT BRECCIAS;
NEUTRON DETECTOR; SOLAR-SYSTEM; NOBLE-GASES
AB The globally-averaged concentrations of radioelements K and Th within Vesta's regolith are determined from gamma ray spectra acquired by Dawn's Gamma Ray and Neutron Detector (GRaND). Spectra measured by GRaND's bismuth germanate (BGO) scintillator, while in close proximity to Vesta, are analyzed. Improvements in data reduction and analysis methods enable detection and quantification of K and Th. Ample precision is achieved using the entire data set acquired by Dawn during 5 months of low-altitude operations. A simple, analytic model, which can be applied to measurements of Vesta and Ceres, is used to determine radioelement concentrations from measured counting rates. Systematic errors in the analysis are evaluated using simulated gamma ray spectra for representative vestan meteorite compositions. Concentrations of K and Th within Vesta's global regolith, measured by GRaND, are consistent with eucrite-rich howardite, and are distinct from most achondrites, all chondrites, and Mars meteorites. The K/Th ratio of Vesta (900 +/- 400) is similar to the average ratio for howardite (approximately 1200). These radioelement data, along with major element ratios determined by nuclear spectroscopy, strongly support the hypothesis that Vesta is the parent body of the HEDs. The depletion of moderately-volatile elements implied by the measured K/Th ratio is consistent with early accretion of Vesta from a hot, incompletely condensed solar nebula and/or, less likely, subsequent removal of volatiles by energetic collisions or degassing of magmas. (C) 2015 The Authors. Published by Elsevier Inc.
C1 [Prettyman, T. H.; Yamashita, N.; Reedy, R. C.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[McSween, H. Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Mittlefehldt, D. W.] NASA Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA.
[Hendricks, J. S.] TechSource Inc, Los Alamos, NM 87544 USA.
[Toplis, M. J.] CNRS Unive Toulouse, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
RP Prettyman, TH (reprint author), Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
EM prettyman@psi.edu; yamashita@psi.edu; reedy@psi.edu; mcsween@utk.edu;
david.w.mittlefehldt@nasa.gov; jhendricks@techsource-inc.com;
michael.toplis@irap.omp.eu
OI Reedy, Robert/0000-0002-2189-1303; Prettyman, Thomas/0000-0003-0072-2831
FU NASA Dawn at Vesta Participating Scientist Program; NASA Discovery
Program
FX This work was carried out under contract with the NASA Jet Propulsion
Laboratory, which is operated by the California Institute of Technology
in Pasadena, California. The Dawn mission is led by the University of
California, Los Angeles under the auspices of the NASA Discovery
Program. GRaND is managed by the Planetary Science Institute. Funding
for D.W.M. and R.C.R. was provided by the NASA Dawn at Vesta
Participating Scientist Program. We greatly appreciate comments by Larry
R. Nittler and an anonymous reviewer, which helped improve the
manuscript.
NR 93
TC 2
Z9 2
U1 5
U2 13
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 OCT
PY 2015
VL 259
SI SI
BP 39
EP 52
DI 10.1016/j.icarus.2015.05.035
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR3UL
UT WOS:000361258500004
ER
PT J
AU Combe, JP
McCord, TB
McFadden, LA
Ieva, S
Tosi, F
Longobardo, A
Frigeri, A
De Sanctis, MC
Ammannito, E
Ruesch, O
Palomba, E
Fulchignoni, M
Raymond, CA
Russell, CT
AF Combe, Jean-Philippe
McCord, Thomas B.
McFadden, Lucy A.
Ieva, Simone
Tosi, Federico
Longobardo, Andrea
Frigeri, Alessandro
De Sanctis, Maria Cristina
Ammannito, Eleonora
Ruesch, Ottaviano
Palomba, Ernesto
Fulchignoni, Marcello
Raymond, Carol A.
Russell, Christopher T.
TI Composition of the northern regions of Vesta analyzed by the Dawn
mission
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids, composition; Mineralogy; Spectroscopy
ID ASTEROID 4 VESTA; MINERAL ABSORPTION FEATURES; REFLECTANCE SPECTROSCOPY;
HYPERSPECTRAL IMAGES; DARK MATERIAL; HED METEORITES; GEOLOGIC MAP;
SOUTH-POLE; GAMMA-RAY; SURFACE
AB The surface composition of the northern regions of Vesta, observed by the Dawn spacecraft, offers the possibility to test several hypotheses related to impact-related processes. We used mostly imaging spectrometry in the visible and near infrared to assess the distribution of mafic lithologies, hydrated components and albedo properties, and use the link with howardite, eucrite and diogenite meteorites (HEDs) to investigate the origin of those materials. We established that Rheasilvia ejecta reached part of the northern regions, and have a diogenitic-rich composition characteristic of the lower crust. Investigations of the antipodes of the two major impact basins (Rheasilvia and Veneneia) did not reveal any correlation between geographic location, geological features and the surface composition. The northern wall of Mamilia crater, which is one of the freshest craters above 22 degrees N, contains relatively pure eucritic-rich, diogenitic-rich and dark, hydrated materials, which are representative of the rest of the northern regions (and most of Vesta), with the exception of an olivine-like component found in Bellicia crater by Ammannito et al. (Ammannito, E. et al. [2013a]. Nature 504(7478), 122-125). We determined that similar types of materials are found in various proportions over a large region, including Bellicia, Arruntia and Pomponia craters, and their origin does not seem to be related to Rheasilvia ejecta. These materials are hydrated, which could indicate an exogenous origin, and not as dark as expected for carbonaceous chondrites, which likely compose the majority of dark hydrated materials on Vesta. Spectral mixture analysis reveals that mixtures of pyroxenes (hypersthene, pigeonite and diopside) could offer an alternative interpretation to olivine in this area. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Combe, Jean-Philippe; McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA.
[McFadden, Lucy A.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ieva, Simone; Fulchignoni, Marcello] Observ Paris, F-92195 Meudon, France.
[Ieva, Simone] INAF, Osserv Astron Roma, Rome, Italy.
[Tosi, Federico; Longobardo, Andrea; Frigeri, Alessandro; De Sanctis, Maria Cristina; Ammannito, Eleonora; Palomba, Ernesto] Ist Astrofis & Planetol Spaziali Ist Nazl Astrofi, I-00133 Rome, Italy.
[Ammannito, Eleonora; Russell, Christopher T.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
[Ruesch, Ottaviano] Univ Munster, Inst Planetol, D-48149 Munster, Germany.
[Raymond, Carol A.] Jet Prop Lab, Pasadena, CA 91109 USA.
RP Combe, JP (reprint author), Bear Fight Inst, 22 Fiddlers Rd,POB 667, Winthrop, WA 98862 USA.
EM jean-philippe_combe@bearfightinstitute.com
RI Frigeri, Alessandro/F-2151-2010;
OI Tosi, Federico/0000-0003-4002-2434; Frigeri,
Alessandro/0000-0002-9140-3977; McFadden, Lucy/0000-0002-0537-9975; De
Sanctis, Maria Cristina/0000-0002-3463-4437; Palomba,
Ernesto/0000-0002-9101-6774
FU NASA Dawn mission through University of California, Los Angeles
[2090-S-MB516]
FX The funding for this research was provided under the NASA Dawn mission
through a subcontract 2090-S-MB516 from the University of California,
Los Angeles. The VIR instrument and VIR team were founded by ASI
(Italian Space Agency) and INAF (Istituto Nazionale di Astrofisica).
NR 88
TC 11
Z9 12
U1 2
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD OCT
PY 2015
VL 259
SI SI
BP 53
EP 71
DI 10.1016/j.icarus.2015.04.026
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR3UL
UT WOS:000361258500005
ER
PT J
AU Longobardo, A
Palomba, E
De Sanctis, MC
Zinzi, A
Scully, JEC
Capaccioni, F
Tosi, F
Zambon, F
Ammannito, E
Combe, JP
Raymond, CA
Russell, CT
AF Longobardo, Andrea
Palomba, Ernesto
De Sanctis, Maria Cristina
Zinzi, Angelo
Scully, Jennifer E. C.
Capaccioni, Fabrizio
Tosi, Federico
Zambon, Francesca
Ammannito, Eleonora
Combe, Jean-Philippe
Raymond, Carol A.
Russell, Cristopher T.
TI Mineralogical and spectral analysis of Vesta's Gegania and Lucaria
quadrangles and comparative analysis of their key features
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids, surfaces; Spectroscopy; Mineralogy; Tectonics
ID ASTEROID 4 VESTA; DARK MATERIAL; 21 LUTETIA; INFRARED SPECTROMETER;
IMAGING SPECTROMETER; NORTHERN-HEMISPHERE; DAWN MISSION; SURFACE;
IMPACT; CRATERS
AB This work is aimed at developing and interpreting infrared albedo, pyroxene and OH band depths, and pyroxene band center maps of Vesta's Gegania and Lucaria quadrangles, obtained from data provided by the Visible and InfraRed (VIR) mapper spectrometer on board NASA's Dawn spacecraft.
The Gegania and Lucaria quadrangles span latitudes from 22 degrees S to 22 degrees N and longitudes from 0 degrees E to 144 degrees E. The mineralogical and spectral maps identify two large-scale units on this area of Vesta, which extend eastwards and westward of about 60 degrees E, respectively. The two regions are not associated to large-scale geological units, which have a latitudinal distribution rather than longitudinal, but are defined by different contents of carbonaceous chondrites (CC): the eastern region, poor in CCs, is brighter and OH-depleted, whereas the western one, rich in CCs, is darker and OH-enriched.
A detailed analysis of the small-scale units in these quadrangles is also performed. Almost all the units show the typical correspondence between high albedo, deep pyroxene bands, short band centers and absence of OH and vice versa. Only a few exceptions occur, such as the ejecta from the Aelia crater, where dark and bright materials are intimately mixed.
The most characteristic features of these quadrangles are the equatorial troughs and the Lucaria tholus.
The equatorial troughs consist of graben, i.e. a depression limited by two conjugate faults. The graben do not present their own spectral signatures, but spectral parameters similar to their surroundings, in agreement to their structural origin. This is observed also in graben outside the Gegania and Lucaria quadrangles. However, it is possible to observe other structural features, such as tectonic grooves, characterized by a changing composition and hence an albedo variation. This result is confirmed not only by mineralogical maps of Vesta, but also by analyzing the VIRTIS-Rosetta observations of Lutetia. The albedo change is instead a typical behavior of geomorphic grooves. Finally, ridges are characterized by a bluer color and, in some cases, shorter band centers than their surroundings, suggesting that they are composed of fresher materials.
We also performed a comparative analysis between the three tholi of Vesta, i.e. Lucaria (which gives the name to its quadrangle), Aricia (in the Marcia quadrangle) and Brumalia (Numisia quadrangle). Whereas Brumalia tholus is a young magmatic intrusion, the absence of diogenites, the low albedo, and the orientation of Aricia and Lucaria tholi suggest that they are older features, which are covered by dark materials and therefore experienced a different geological history than Brumalia. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Longobardo, Andrea; Palomba, Ernesto; De Sanctis, Maria Cristina; Capaccioni, Fabrizio; Tosi, Federico; Zambon, Francesca] INAF Ist Astrofis & Planetol Spaziali IAPS, I-00133 Rome, Italy.
[Zinzi, Angelo] ASI ASI Sci Data Ctr ASDC, I-00133 Rome, Italy.
[Zinzi, Angelo] INAF Osservatorio Astron Roma OAR, I-00040 MON Monte Porzio Catone, RM, Italy.
[Scully, Jennifer E. C.; Ammannito, Eleonora; Russell, Cristopher T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Combe, Jean-Philippe] Bear Fight Inst, Winthrop, WA 98862 USA.
[Raymond, Carol A.] CALTECH, JPL, Pasadena, CA 91109 USA.
RP Longobardo, A (reprint author), INAF Ist Astrofis & Planetol Spaziali IAPS, Via Fosso del Cavaliere, I-00133 Rome, Italy.
EM andrea.longobardo@iaps.inaf.it
OI De Sanctis, Maria Cristina/0000-0002-3463-4437; Capaccioni,
Fabrizio/0000-0003-1631-4314; ZINZI, Angelo/0000-0001-5263-5348;
Palomba, Ernesto/0000-0002-9101-6774; Tosi,
Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592
FU Dawn Science, Instrument, and Operations Teams; FC Science Team; ASI;
NASA; Italian Space Agency-ASI
FX VIR is funded by the Italian Space Agency-ASI and was developed under
the leadership of INAF-Istituto di Astrofisica e Planetologia Spaziali,
Rome, Italy. The instrument was built by Selex-Galileo, Florence, Italy.
The authors acknowledge the support of the Dawn Science, Instrument, and
Operations Teams and of the FC Science Team. This work was supported by
ASI and NASA.
NR 63
TC 7
Z9 7
U1 1
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD OCT
PY 2015
VL 259
SI SI
BP 72
EP 90
DI 10.1016/j.icarus.2015.04.031
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR3UL
UT WOS:000361258500006
ER
PT J
AU De Sanctis, MC
Combe, JP
Ammannito, A
Frigeri, A
Longobardo, A
Palomba, E
Tosi, F
Zambon, F
Stephan, K
Raymond, CA
Russell, CT
AF De Sanctis, M. C.
Combe, J. -P
Ammannito, A.
Frigeri, A.
Longobardo, A.
Palomba, E.
Tosi, F.
Zambon, F.
Stephan, K.
Raymond, C. A.
Russell, C. T.
TI Eucritic crust remnants and the effect of in-falling hydrous
carbonaceous chondrites characterizing the composition of Vesta's Marcia
region
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Spectroscopy; Mineralogy
ID ASTEROID 4 VESTA; SPACE-TELESCOPE IMAGES; DAWN MISSION;
SPECTRAL-ANALYSIS; DARK MATERIAL; MINERALOGICAL CHARACTERIZATION;
REFLECTANCE PROPERTIES; IMAGING SPECTROMETER; HYDRATED MATERIAL; PARENT
BODY
AB The equatorial Marcia quadrangle region is characterized by the large, relatively young impact craters Marcia and Calpurnia and their surrounding dark ejecta field, a hill with a dark-rayed crater named Aricia Tholus, and an unusual diffuse material surrounding the impact crater Octavia. The spectral analysis indicates that while this region is relatively uniform in the pyroxene band centers, it instead shows large differences in pyroxene band depths and reflectance. A large variation of reflectance is seen in the quadrangle: bright and dark materials are present as diffuse material, and as concentrated spots and outcrops. Moreover, OH signature is pervasive in the quadrangle, with a few exceptions. The region, especially the Marcia ejecta field, is characterized by spectra showing the 2 urn band shifted at long wavelengths. This is commonly associated with eucritic material, believed to have crystallized as lava on Vesta's surface or within relatively shallow-level dikes and plutons, thus suggesting that this region is a remnant of the old Vestan basaltic crust. However, other characteristics of the spectra do not fully fit the eucritic composition, indicating an alternative explanation for the band center distribution, including the presence of carbonaceous chondritic material mixed with the native Vestan pyroxene.
The detailed mineralogical analysis of the Marcia quadrangle indicates that this quadrangle is the result of the mixture of the Vestan "endogenic" minerals with the "exogenic" carbonaceous chondrites. The stratigraphic units around Marcia clearly show the bright, uncontaminated material interlaced and mixed with the dark material that contains a strong OH signature. Only few small areas can be considered as representative of the old Vestan original material. (C) 2015 Elsevier Inc. All rights reserved.
C1 [De Sanctis, M. C.; Ammannito, A.; Frigeri, A.; Longobardo, A.; Palomba, E.; Tosi, F.; Zambon, F.] Ist Astrofis & Planetol Spaziali, INAF, Area Ric Tor Vergata, I-00133 Rome, Italy.
[Combe, J. -P] Bear Fight Inst, Winthrop, WA 98862 USA.
[Ammannito, A.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Stephan, K.] Inst Planetary Res, D-12489 Berlin, Germany.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP De Sanctis, MC (reprint author), Ist Astrofis & Planetol Spaziali, INAF, Area Ric Tor Vergata, I-00133 Rome, Italy.
EM mariacristina.desanctis@iaps.inaf.it
RI Frigeri, Alessandro/F-2151-2010;
OI Frigeri, Alessandro/0000-0002-9140-3977; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Palomba, Ernesto/0000-0002-9101-6774;
Tosi, Federico/0000-0003-4002-2434; Zambon,
Francesca/0000-0002-4190-6592
FU Italian Space Agency; Dawn Science, Instrument, and Operations Teams;
NASA
FX VIR is funded by the Italian Space Agency and was developed under the
leadership of INAF-Istituto di Astrofisica e Planetologia Spaziali,
Rome, Italy. The instrument was built by Selex-ES, Florence, Italy. The
authors acknowledge the support of the Dawn Science, Instrument, and
Operations Teams. We thank the FC team for providing the FC images and
DLR team for the FC mosaics. This work was supported by the Italian
Space Agency. A portion of this work was performed at the Jet Propulsion
Laboratory under contract with NASA.
NR 79
TC 5
Z9 5
U1 1
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD OCT
PY 2015
VL 259
SI SI
BP 91
EP 115
DI 10.1016/j.icarus.2015.05.014
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR3UL
UT WOS:000361258500007
ER
PT J
AU Frigeri, A
De Sanctis, MC
Ammannito, E
Buczkowski, D
Combe, JP
Tosi, F
Zambon, F
Rocchini, D
Jaumann, R
Raymond, CA
Russell, CT
AF Frigeri, A.
De Sanctis, M. C.
Ammannito, E.
Buczkowski, D.
Combe, J. P.
Tosi, F.
Zambon, F.
Rocchini, D.
Jaumann, R.
Raymond, C. A.
Russell, C. T.
TI Mineralogic mapping of the Av-9 Numisia quadrangle of Vesta
SO ICARUS
LA English
DT Article
DE Asteroid vests; Mineralogy; Geological processes; Data reduction
techniques
ID ASTEROID 4 VESTA; SPECTRAL REFLECTANCE; HED METEORITES; DARK MATERIAL;
DAWN; PYROXENES; HETEROGENEITY; SPECTROMETER; SPECTROSCOPY; DIOGENITES
AB In this manuscript we present the mineralogic mapping of the Av-9 Numisia quadrangle of Vesta using the most up-to-date data from the NASA-Dawn mission.
This quadrangle is located in Vesta's equatorial zone (22 south to 22 north, 218 to 288 east, in Claudia coordinate system) and takes its name from the impact crater Numisia. The main feature, which dominates the quadrangle, is the Vestalia Terra plateau, a topographic high about 10 km above the surrounding areas. To the south, this region fades into the Rheasilvia basin, while to the north it is bounded by the steep scarp of Postumia basin.
The Visible and Infrared mapping spectrometer (VIR) onboard NASA/Dawn provided the main data source for this work, at an unprecedented level of spatial and spectral resolution. In particular we are using spectral parameters to synthesize characteristics of the whole spectra into a single value. Pyroxene-related spectral parameters allow for the detection of lower crust or mantle material (diogenites) and upper crust material (eucrites) in the study area.
The combined analysis of albedo from the Framing Camera, the geologic map and the spectroscopic data offer an interesting opportunity to understand better the surface features of this region of Vesta, and their evolution.
Numisia, Cornelia, Fabia, Teia and Drusilla are the main craters in the study area, rich in bright and dark material outcrops, pitted terrains and OH-rich materials.
Using the spectral parameters we demonstrate that the internal composition of Vestalia Terra is mainly diogenite-rich howardite, as shown by materials excavated by Cornelia and Fabia, and the composition of the slope north of Vestalia Terra. This agrees with the strong positive Bouguer Anomaly observed in the area, indicating a higher density of these features in relation to the surrounding areas.
Besides the recently published works based on gravimetric modeling and geologic interpretation, the mineralogic mapping presented herein gives an additional contribution, in order to depict a more complete geologic history of the Numisia quadrangle of Vesta. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Frigeri, A.; De Sanctis, M. C.; Tosi, F.; Zambon, F.] IAPS, Ist Nazl Astrofis INAF, I-00133 Rome, Italy.
[Buczkowski, D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Jaumann, R.] German Aerosp Ctr, Inst Planetary Res, Berlin, Germany.
[Combe, J. P.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ammannito, E.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Rocchini, D.] Fdn Edmund Mach, Res & Innovat Ctr, Dept Biodivers & Mol Ecol, I-38010 San Michele All Adige, TN, Italy.
RP Frigeri, A (reprint author), IAPS, Ist Nazl Astrofis INAF, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
EM alessandro.frigeri@iaps.inaf.it
RI Frigeri, Alessandro/F-2151-2010;
OI Frigeri, Alessandro/0000-0002-9140-3977; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Rocchini, Duccio/0000-0003-0087-0594;
Tosi, Federico/0000-0003-4002-2434; Zambon,
Francesca/0000-0002-4190-6592
NR 39
TC 5
Z9 5
U1 2
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 OCT
PY 2015
VL 259
SI SI
BP 116
EP 128
DI 10.1016/j.icarus.2015.07.029
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR3UL
UT WOS:000361258500008
ER
PT J
AU Tosi, F
Frigeri, A
Combe, JP
Zambon, F
De Sanctis, MC
Ammannito, E
Longobardo, A
Hoffmann, M
Nathues, A
Garry, WB
Blewett, DT
Pieters, CM
Palomba, E
Stephan, K
McFadden, LA
McSween, HY
Russell, CT
Raymond, CA
AF Tosi, F.
Frigeri, A.
Combe, J. -Ph.
Zambon, F.
De Sanctis, M. C.
Ammannito, E.
Longobardo, A.
Hoffmann, M.
Nathues, A.
Garry, W. B.
Blewett, D. T.
Pieters, C. M.
Palomba, E.
Stephan, K.
McFadden, L. A.
McSween, H. Y.
Russell, C. T.
Raymond, C. A.
CA Dawn Sci Team
TI Mineralogical analysis of the Oppia quadrangle of asteroid (4) Vesta:
Evidence for occurrence of moderate-reflectance hydrated minerals
SO ICARUS
LA English
DT Article
DE Asteroids, surfaces; Asteroid Vesta; Spectrophotometry; Infrared
observations
ID HUBBLE-SPACE-TELESCOPE; SPECTRAL-ANALYSIS; IMPACT CRATERS; CLEMENTINE
DATA; DARK MATERIAL; DAWN MISSION; SPECTROMETER; OLIVINE; SURFACE;
REGION
AB Quadrangle Av-10 'Oppia' is one of five quadrangles that cover the equatorial region of asteroid (4) Vesta. This quadrangle is notable for the broad, spectrally distinct ejecta that extend south of the Oppia crater. These ejecta exhibit the steepest ('reddest') visible spectral slope observed across the asteroid and have distinct color properties as seen in multispectral composite images. Compared to previous works that focused on the composition and nature of unusual ('orange') ejecta found on Vesta, here we take into account a broader area that includes several features of interest, with an emphasis on mineralogy as inferred from data obtained by Dawn's Visible InfraRed mapping spectrometer (VIR). Our analysis shows that the older northern and northeastern part of Av-10 is dominated by howardite-like material, while the younger southwestern part, including Oppia and its ejecta blanket, has a markedly eucritic mineralogy. The association of the mineralogical information with the geologic and topographic contexts allows for the establishment of relationships between the age of the main formations observed in this quadrangle and their composition. A major point of interest in the Oppia quadrangle is the spectral signature of hydrous material seen at the local scale. This material can be mapped by using high-resolution VIR data, combined with multispectral image products from the Dawn Framing Camera (FC) so as to enable a clear correlation with specific geologic features. Hydrated mineral phases studied previously on Vesta generally correlate with low-albedo material delivered by carbonaceous asteroids. However, our analysis shows that the strongest OH signature in Av-10 is found in a unit west of Oppia, previously mapped as 'light mantle material' and showing moderate reflectance and a red visible slope. With the available data we cannot yet assess the presence of water in this material. However, we offer a possible explanation for its origin. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Tosi, F.; Frigeri, A.; Zambon, F.; De Sanctis, M. C.; Ammannito, E.; Longobardo, A.; Palomba, E.] INAF IAPS, I-00133 Rome, Italy.
[Combe, J. -Ph.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Ammannito, E.; Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Hoffmann, M.; Nathues, A.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
[Garry, W. B.; McFadden, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Blewett, D. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Pieters, C. M.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
[Stephan, K.] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[McSween, H. Y.] Univ Tennesse, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Raymond, C. A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Raymond, C. A.] CALTECH, Pasadena, CA 91109 USA.
RP Tosi, F (reprint author), INAF IAPS, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
EM federico.tosi@iaps.inaf.it
RI Frigeri, Alessandro/F-2151-2010;
OI Frigeri, Alessandro/0000-0002-9140-3977; McFadden,
Lucy/0000-0002-0537-9975; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Palomba, Ernesto/0000-0002-9101-6774;
Tosi, Federico/0000-0003-4002-2434; Zambon,
Francesca/0000-0002-4190-6592
FU ASI-INAF [I/004/12/0]; NASA Dawn at Vesta Participating Scientist
program; Italian Space Agency (ASI)
FX This work was supported by the Italian Space Agency (ASI), ASI-INAF
Contract I/004/12/0. The authors thank the Dawn Science, Operation and
Instrument Teams for a successful Dawn at Vesta mission. D.T. Blewett
received support from the NASA Dawn at Vesta Participating Scientist
program. The VIR instrument was developed under the leadership of INAF,
Italy's National Institute for Astrophysics, Rome. The instrument was
built by SELEX-Galileo, Florence, Italy. We thank Jennifer Scully and
Sharon Uy for their assistance in revising the manuscript. Dawn datasets
are publicly available at the Planetary Data System Small Bodies Node
(http://pdssbn.astro.umd.edu/).
NR 62
TC 7
Z9 7
U1 3
U2 5
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 OCT
PY 2015
VL 259
SI SI
BP 129
EP 149
DI 10.1016/j.icarus.2015.05.018
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR3UL
UT WOS:000361258500009
ER
PT J
AU McFadden, LA
Combe, JP
Ammannito, E
Frigeri, A
Stephan, K
Longobardo, A
Palomba, E
Tosi, F
Zambon, F
Krohn, K
De Sanctis, MC
Reddy, V
Le Corre, L
Nathues, A
Pieters, CM
Prettyman, TH
Raymond, CA
Russell, CT
AF McFadden, L. A.
Combe, J. -P.
Ammannito, E.
Frigeri, A.
Stephan, K.
Longobardo, A.
Palomba, E.
Tosi, F.
Zambon, F.
Krohn, K.
De Sanctis, M. C.
Reddy, V.
Le Corre, L.
Nathues, A.
Pieters, C. M.
Prettyman, T. H.
Raymond, C. A.
Russell, C. T.
TI Vesta's Pinaria region: Original basaltic achondrite material derived
from mixing upper and lower crust
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids, composition; Asteroids, surfaces; Mineralogy;
Meteorites
ID HUBBLE-SPACE-TELESCOPE; ASTEROID 4 VESTA; DAWN MISSION; REFLECTANCE
SPECTRA; DARK MATERIAL; PARENT BODY; SPECTROMETER; OLIVINE;
HETEROGENEITY; SPECTROSCOPY
AB Analysis of data from the Dawn mission shows that the Pinaria region of Vesta spanning a portion of the rim of the Rheasilvia basin is bright and anhydrous. Reflectance spectra, absorption band centers, and their variations, cover the range of pyroxenes from diogenite-rich to howardite and eucrite compositions, with no evidence of olivine in this region. By examining band centers and depths of the floor, walls and rims of six major craters in the region, we find a lane of diogenite-rich material next to howardite-eucrite material that does not follow the local topography. The source of this material is not clear and is probably ejecta from post-Rheasilvia impacts. Material of a howardite-eucrite composition originating from beyond the Rheasilvia basin is evident on the western edge of the region. Overall, the Pinaria region exposes the complete range of basaltic achondrite parent body material, with little evidence of contamination of non-basaltic achondrite material. With both high reflectance and low abundance of hydrated material, this region of Vesta may be considered the "Pinaria desert". Published by Elsevier Inc.
C1 [McFadden, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Combe, J. -P.] Bearfight Inst, Winthrop, WA 98826 USA.
[Ammannito, E.; Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Frigeri, A.; Longobardo, A.; Palomba, E.; Tosi, F.; Zambon, F.; De Sanctis, M. C.] INAF IAPS, I-00133 Rome, Italy.
[Stephan, K.; Krohn, K.] German Aerosp Ctr DLR, D-12489 Berlin, Germany.
[Nathues, A.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
[Pieters, C. M.] Brown Univ, Providence, RI 02912 USA.
[Reddy, V.; Le Corre, L.; Prettyman, T. H.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP McFadden, LA (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Code 693,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM lucy.mcfadden@nasa.gov
RI Frigeri, Alessandro/F-2151-2010;
OI Frigeri, Alessandro/0000-0002-9140-3977; McFadden,
Lucy/0000-0002-0537-9975; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Prettyman, Thomas/0000-0003-0072-2831; Le
Corre, Lucille/0000-0003-0349-7932; Palomba,
Ernesto/0000-0002-9101-6774; Tosi, Federico/0000-0003-4002-2434; Zambon,
Francesca/0000-0002-4190-6592
FU Italian Space Agency-ASI; Max Planck Society; German Space Agency, DLR;
NASA's Dawn at Vesta Participating Scientist Program [NNX10AR56G]; NASA
[NNM05AA86C]; Dawn mission through NASA's Discovery Program
FX VIR is funded by the Italian Space Agency-ASI and was developed under
the leadership of INAF-Istituto di Astrofisica e Planetologia Spaziali,
Rome-Italy. The Framing Camera project is financially supported by the
Max Planck Society and the German Space Agency, DLR. Members of those
institutions acknowledge their support. This work was supported by the
Dawn mission through NASA's Discovery Program, NASA's Dawn at Vesta
Participating Scientist Program through Grants NNX10AR56G to Planetary
Science Institute. Part of this work was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA to UCLA NASA contract number, NNM05AA86C. The Dawn
Flight Team made the observations possible and we thank them for their
superior driving and operations implementation. We greatly appreciate
assistance with graphics by Bike Kersten and Jay Friedlander. And we
thank Beth Clark and an anonymous reviewer for their thorough and
socratic review and suggestions that guided the revision and improvement
of the manuscript. We remember Angioletta Coriadini, our deceased
colleague, through study of the crater Angioletta named in her honor.
NR 54
TC 5
Z9 5
U1 0
U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD OCT
PY 2015
VL 259
SI SI
BP 150
EP 161
DI 10.1016/j.icarus.2015.07.003
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR3UL
UT WOS:000361258500010
ER
PT J
AU Stephan, K
Jaumann, R
De Sanctis, MC
Ammannito, E
Krohn, K
Otto, K
Tosi, F
Combe, JP
Roatsch, T
Matz, KD
McFadden, LA
Preusker, F
Raymond, CA
Russell, CT
AF Stephan, Katrin
Jaumann, Ralf
De Sanctis, Maria C.
Ammannito, Eleonora
Krohn, Katrin
Otto, Katharina
Tosi, Federico
Combe, Jean-Phillipe
Roatsch, Thomas
Matz, Klaus-Dieter
McFadden, Lucy A.
Preusker, Frank
Raymond, Carol A.
Russell, Chris T.
TI The Sextilia-region on Asteroid 4Vesta-Stratigraphy and variegation
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Spectroscopy; Asteroids, composition; Asteroids,
surfaces
ID FRAMING CAMERA IMAGES; 4 VESTA; REFLECTANCE SPECTRA;
SURFACE-COMPOSITION; HED METEORITES; DARK MATERIAL; DAWN MISSION;
SOLAR-SYSTEM; SPECTROMETER; DIOGENITES
AB Mapping Vesta' surface composition in the Sextilia region offers the unique possibility to investigate stratigraphic relationship of the surface compounds throughout the transition from Rheasilvia, Vesta's prominent impact basin, to Vesta's northern equatorial region. The VIR data point to an upper eucrite-dominated layer overlaying extended deposits of diogenite in the subsurface, which reaches the surface at Matronalia Rupes, the uplifted rim of the Rheasilvia impact structure. The dominance of diogenite in Matronalia Rupes suggests the existence of an extended diogenite-rich layer and supports the magma-ocean model as the most plausible formation model for Vesta's interior. Local enrichment of diogenite outside of the Rheasilvia impact basin are interpreted as outcrops of diogenite-dominated breccia excavated during the Rheasilvia impact event and re-excavated by more recent impacts. On the contrary, the asymmetry in the distribution of diogenite-rich outcrops in the norther parts, i.e., the depletion of these deposits in the Veneneia region, is at odds with the equally distributed plutonic intrusions of diogenite-rich material as proposed in the serial magmatism model but could be explained by an uneven distribution of its ejecta on Vesta's surface due to an oblique Rheasilvia impact. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Stephan, Katrin; Jaumann, Ralf; Krohn, Katrin; Otto, Katharina; Roatsch, Thomas; Matz, Klaus-Dieter; Preusker, Frank] DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[Jaumann, Ralf] Free Univ Berlin, Inst Geosci, D-12249 Berlin, Germany.
[De Sanctis, Maria C.; Tosi, Federico] Ist Astrofis & Planetol Spaziali, INAF, I-00133 Rome, Italy.
[Ammannito, Eleonora; Russell, Chris T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90096 USA.
[Combe, Jean-Phillipe] Bear Fight Inst, Winthrop, WA 98862 USA.
[McFadden, Lucy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Stephan, K (reprint author), DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany.
EM Katrin.Stephan@dlr.de
OI McFadden, Lucy/0000-0002-0537-9975; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Tosi, Federico/0000-0003-4002-2434
FU DAWN Science, Instrument, and Operation Teams; DLR; NASA
FX We acknowledge the support of the DAWN Science, Instrument, and
Operation Teams. We also thank the instrument teams at the German
Aerospace Center (DLR), Italian National Institute for Astrophysics
(INAF) Max Planck Institute and Planetary Science Institute for the
acquisition and processing of Dawn data used in this work. This work was
supported by DLR and NASA.
NR 87
TC 3
Z9 3
U1 0
U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD OCT
PY 2015
VL 259
SI SI
BP 162
EP 180
DI 10.1016/j.icarus.2015.05.016
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR3UL
UT WOS:000361258500011
ER
PT J
AU Zambon, F
Frigeri, A
Combe, JP
Tosi, F
Longobardo, A
Ammannito, E
De Sanctis, MC
Blewett, DT
Scully, J
Palomba, E
Denevi, B
Yingst, A
Russell, CT
Raymond, CA
AF Zambon, F.
Frigeri, A.
Combe, J. -Ph.
Tosi, F.
Longobardo, A.
Ammannito, E.
De Sanctis, M. C.
Blewett, D. T.
Scully, J.
Palomba, E.
Denevi, B.
Yingst, A.
Russell, C. T.
Raymond, C. A.
TI Spectral analysis of the quadrangles Av-13 and Av-14 on Vesta
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Mineralogy; Spectroscopy
ID ASTEROID 4 VESTA; DAWN FRAMING CAMERA; REFLECTANCE SPECTRA;
INFRARED-SPECTRA; DARK MATERIAL; SURFACE; METEORITES; MINERALOGY;
PYROXENES; OLIVINE
AB The Av-13 (Tuccia) and Av-14 (Urbinia) quadrangles are located in the south-west region of Vesta. They are characterized by a large topographic variability, from the highest (Vestalia terra highlands) to the lowest (Rheasilvia basin). Many geological units in these quadrangles are not associated with mineralogical variability, as shown by the color-composite maps. Maps of mafic absorption band-center position reveal that the principal lithology is eucrite-rich howardite, but diogenite-rich howardite areas are also present, corresponding to particular features such as Antonia and Justina craters, which are characterized by strong mafic absorptions. These quadrangles, especially Urbinia, contain many bright ejecta, such as those of Tuccia crater, which are the highest reflectance materials on Vesta (Zambon et al., 2014). Dark areas are present and correspond to regions with deeper OH-signature. The two quadrangles contain many vertical ridge crests associated with the Rheasilvia impact. These ridges do not show mineralogical differences with respect to their surroundings, but have a distinctive appearance in color-ratio composite images. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Zambon, F.; Frigeri, A.; Tosi, F.; Longobardo, A.; De Sanctis, M. C.; Palomba, E.] INAF IAPS, I-00133 Rome, Italy.
[Combe, J. -Ph.] Bearfight Inst, Winthrop, WA 98862 USA.
[Ammannito, E.; Blewett, D. T.; Russell, C. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Scully, J.; Denevi, B.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Yingst, A.] PSI, Tucson, AZ USA.
[Raymond, C. A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Raymond, C. A.] CALTECH, Pasadena, CA 91109 USA.
RP Zambon, F (reprint author), INAF IAPS, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
EM francesca.zambon@iaps.inaf.it
RI Denevi, Brett/I-6502-2012; Frigeri, Alessandro/F-2151-2010;
OI Palomba, Ernesto/0000-0002-9101-6774; Tosi,
Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592;
Denevi, Brett/0000-0001-7837-6663; Frigeri,
Alessandro/0000-0002-9140-3977; De Sanctis, Maria
Cristina/0000-0002-3463-4437
FU Italian Space Agency-ASI; INAF-Istituto di Astrofisica e Planetologia
Spaziale, Rome, Italy; Dawn Science, Instrument, and Operations Teams;
ASI; NASA's
FX VIR is funded by the Italian Space Agency-ASI and was developed under
the leadership of INAF-Istituto di Astrofisica e Planetologia Spaziale,
Rome, Italy. The instrument was built by Selex-Galileo, Florence-Italy.
The authors acknowledge the support of the Dawn Science, Instrument, and
Operations Teams. This work was supported by ASI and NASA's.
NR 69
TC 7
Z9 7
U1 1
U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD OCT
PY 2015
VL 259
SI SI
BP 181
EP 193
DI 10.1016/j.icarus.2015.05.015
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR3UL
UT WOS:000361258500012
ER
PT J
AU Ammannito, E
De Sanctis, MC
Combe, JP
Frigeri, A
Jaumann, R
Longobardo, A
McSween, HY
Palomba, E
Tosi, F
Raymond, CA
Russell, CT
AF Ammannito, E.
De Sanctis, M. C.
Combe, J. -Ph.
Frigeri, A.
Jaumann, R.
Longobardo, A.
McSween, H. Y.
Palomba, E.
Tosi, F.
Raymond, C. A.
Russell, C. T.
CA Dawn Sci Team
TI Compositional variations in the Vestan Rheasilvia basin
SO ICARUS
LA English
DT Article
DE Mineralogy; Asteroids, composition; Asteroid Vesta; Asteroids, surfaces
ID ASTEROID 4 VESTA; HUBBLE-SPACE-TELESCOPE; DAWN FRAMING CAMERA; MAGMA
OCEAN; PARENT BODY; OLIVINE; SURFACE; HETEROGENEITY; MISSION; MODELS
AB We present and describe the maps of spectral parameters such as pyroxene band centers and depths, reflectance at 1.4 mu m and 2.8 mu m band depth in the Rheasilvia quadrangle. We found a broad anti-correlation between pyroxene band centers and depths while the reflectance is not correlated with the pyroxene spectral parameters. In addition, we found that the Rheasilvia quadrangle is free of OH absorption signatures. We also derived lithological maps with improvements in the spatial resolution with respect to previous lithological maps of the same region. We confirm that the central mound is dominated by eucritic/howarditic pyroxene while diogenitic lithology has been found mainly in a region delineated by Tarpeia, Severina and Mariamne craters. We found small scale variations in the composition of pyroxene. These variations identify lithological units that extend for tens of km, although small units of less than 1 km have also been found. We consider this fact as an indication of a high level of compositional heterogeneity within the Vestan crust. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Ammannito, E.; Russell, C. T.] Univ Calif Los Angeles, Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
[Ammannito, E.; De Sanctis, M. C.; Frigeri, A.; Longobardo, A.; Palomba, E.; Tosi, F.] Ist Astrofis & Planetol Spaziale, INAF, Area Ric Tor Vergata, Rome, Italy.
[Combe, J. -Ph.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Jaumann, R.] DLR, Inst Planetary Res, Berlin, Germany.
[McSween, H. Y.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA.
[McSween, H. Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ammannito, E (reprint author), Univ Calif Los Angeles, Earth Planetary & Space Sci, 595 Charles Young Dr East, Los Angeles, CA 90095 USA.
EM eleonora.ammannito@igpp.ucla.edu
RI Frigeri, Alessandro/F-2151-2010;
OI Frigeri, Alessandro/0000-0002-9140-3977; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Palomba, Ernesto/0000-0002-9101-6774;
Tosi, Federico/0000-0003-4002-2434
FU NASA; Italian Space Agency (ASI) grant; ASI
FX The authors gratefully acknowledge the contribution of the Dawn
Instruments and Operations Teams. This work is supported by NASA through
the Dawn project and by an Italian Space Agency (ASI) grant. The VIR
spectrometer is funded by ASI. It was built by Selex-Galileo, Florence,
Italy and is now managed by INAF - Istituto di Astrofisica e
Planetologia Spaziali, Rome, Italy.
NR 59
TC 2
Z9 2
U1 2
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD OCT
PY 2015
VL 259
SI SI
BP 194
EP 202
DI 10.1016/j.icarus.2015.05.017
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR3UL
UT WOS:000361258500013
ER
PT J
AU Coppa, AC
Kapoor, M
Hornbuckle, BC
Weaver, ML
Noebe, RD
Thompson, GB
AF Coppa, Anne C.
Kapoor, Monica
Hornbuckle, B. Chad
Weaver, Mark L.
Noebe, Ronald D.
Thompson, Gregory B.
TI Influence of Dilute Hf Additions on Precipitation and Martensitic
Transformation in Ni-Ti-Pd Alloys
SO JOM
LA English
DT Article
ID SHAPE-MEMORY ALLOYS; SPECIMEN PREPARATION; PHASE; RICH; MICROSTRUCTURE
AB The effect of Hf (0-1 at.%) additions in a Ni-Ti-Pd alloy on P-phase precipitation and martensitic transformations was studied. The addition of hafnium resulted in the refinement of precipitates with an increase in number density. The overlapping strain fields created due to the decrease in inter-precipitate spacing are suspected to reduce the matrix volume to be less than the critical free volume size needed for the martensitic transformation over the temperature range studied (183-573 K). Hafnium was also found to delay the aging time to achieve peak hardness, suggesting a reduction in growth and coarsening kinetics.
C1 [Coppa, Anne C.; Kapoor, Monica; Hornbuckle, B. Chad; Weaver, Mark L.; Thompson, Gregory B.] Univ Alabama, Dept Met & Mat Engn, Tuscaloosa, AL 35401 USA.
[Noebe, Ronald D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Coppa, AC (reprint author), Univ Alabama, Dept Met & Mat Engn, Box 870202, Tuscaloosa, AL 35401 USA.
EM gthompson@eng.ua.edu
FU NASA [NNX09AO61A]; NASA FAP Aeronautical Sciences Project
FX The authors gratefully acknowledge funding for this research under NASA
grant NNX09AO61A and the NASA FAP Aeronautical Sciences Project. This
study utilized the Central Analytical Facility (CAF), supported by and
located on the campus at The University of Alabama. Special thanks are
given to Drs. Justin Brons and Billie Wang, Mr. Nicholas De Leon, and
Ms. Suzanne Kornegay for technical assistance.
NR 38
TC 0
Z9 0
U1 1
U2 4
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1047-4838
EI 1543-1851
J9 JOM-US
JI JOM
PD OCT
PY 2015
VL 67
IS 10
BP 2244
EP 2250
DI 10.1007/s11837-015-1567-5
PG 7
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering; Mineralogy; Mining & Mineral Processing
SC Materials Science; Metallurgy & Metallurgical Engineering; Mineralogy;
Mining & Mineral Processing
GA CR6WO
UT WOS:000361489100016
ER
PT J
AU Colgan, W
Abdalati, W
Citterio, M
Csatho, B
Fettweis, X
Luthcke, S
Moholdt, G
Simonsen, SB
Stober, M
AF Colgan, William
Abdalati, Waleed
Citterio, Michele
Csatho, Beata
Fettweis, Xavier
Luthcke, Scott
Moholdt, Geir
Simonsen, Sebastian B.
Stober, Manfred
TI Hybrid glacier Inventory, Gravimetry and Altimetry (HIGA) mass balance
product for Greenland and the Canadian Arctic
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Gravimetry; Altimetry; Glacier; Ice sheet; Canada; Greenland; Mass
balance
ID SEA-LEVEL RISE; ICE-SHEET; RECONCILED ESTIMATE; ELEVATION CHANGES;
BASIN-SCALE; SURFACE; GRACE; CAPS; MODEL; DENSITY
AB We present a novel inversion algorithm that generates a mass balance field that is simultaneously consistent with independent observations of glacier inventory derived from optical imagery, cryosphere-attributed mass trends derived from satellite gravimetry, and ice surface elevation trends derived from airborne and satellite altimetty. We use this algorithm to assess mass balance across Greenland and the Canadian Arctic over the Sep-2003 to Oct2009 period at 26 km resolution. We evaluate local algorithm-inferred mass balance against forty in situ point observations. This evaluation yields an RMSE of 0.15 mWE/a, and highlights a paucity of in situ observations from regions of high dynamic mass loss and peripheral glaciers. We assess mass losses of 212 +/- 67 Gt/a to the Greenland ice sheet proper, 38 +/- 11 Gt/a to peripheral glaciers in Greenland, and 42 +/- 11 Gt/a to glaciers in the Canadian Arctic These magnitudes of mass loss are dependent on the gravimetry-derived spherical harmonic mass trend we invert We spatially partition the transient glacier continuity equation by differencing algorithminferred mass balance from modeled surface mass balance, in order to solve the horizontal divergence of ice flux as a residual. This residual ice dynamic field infers flux divergence (or submergent flow) in the ice sheet accumulation area and at tidewater margins, and flux convergence (or emergent flow) in land-terminating ablation areas, which is consistent with continuum mechanics theory. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Colgan, William; Citterio, Michele] Geol Survey Denmark & Greenland, Marine Geol & Glaciol, Copenhagen, Denmark.
[Colgan, William; Abdalati, Waleed] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Csatho, Beata] SUNY Buffalo, Dept Geol, Buffalo, NY 14260 USA.
[Fettweis, Xavier] Univ Liege, Dept Geog, Liege, Belgium.
[Luthcke, Scott] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Moholdt, Geir] Univ Calif San Diego, Scripps Inst Oceanog, San Diego, CA 92103 USA.
[Moholdt, Geir] Norwegian Polar Res Inst, Fram Ctr, Tromso, Norway.
[Simonsen, Sebastian B.] Tech Univ Denmark, DK-2800 Lyngby, Denmark.
[Stober, Manfred] Stuttgart Univ Appl Sci, Stuttgart, Germany.
RP Colgan, W (reprint author), Geol Survey Denmark & Greenland, Marine Geol & Glaciol, Copenhagen, Denmark.
RI Simonsen, Sebastian /F-4791-2013; Colgan, William/H-1570-2014;
OI Simonsen, Sebastian /0000-0001-9569-1294; Colgan,
William/0000-0001-6334-1660; Fettweis, Xavier/0000-0002-4140-3813
FU NASA [NNX10AR76G]; DFF [FNU 11-115166]; NSF [CNS-0821794]; University of
Colorado Boulder; PROMICE and GlacioBasis; Danish Energy Agency
FX This work was funded by NASA award NNX10AR76G and DFF award FNU
11-115166. This work utilized the Janus supercomputer, which is
supported by NSF award CNS-0821794 and the University of Colorado
Boulder. The Janus supercomputer is a joint effort of the University of
Colorado Boulder, the University of Colorado Denver and the National
Center for Atmospheric Research. W.C. thanks Joel Frahm for his
continued assistance working with Janus. M.C. was supported by PROMICE
and GlacioBasis with funds from the Danish Energy Agency. We thank Ken
Jezek for sharing his field data and reviewing our interpretation of the
mass balance of the Ohio State University clusters in South Greenland.
We also thank two anonymous reviewers, whose insightful comments greatly
improved this manuscript. Dorothy Hall served as our dedicated
scientific editor.
NR 68
TC 2
Z9 2
U1 7
U2 39
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 OCT
PY 2015
VL 168
BP 24
EP 39
DI 10.1016/j.rse.2015.06.016
PG 16
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CR5SY
UT WOS:000361405500003
ER
PT J
AU Duncanson, LI
Dubayah, RO
Cook, BD
Rosette, J
Parker, G
AF Duncanson, L. I.
Dubayah, R. O.
Cook, B. D.
Rosette, J.
Parker, G.
TI The importance of spatial detail: Assessing the utility of individual
crown information and scaling approaches for lidar-based biomass density
estimation
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Lidar; Forest; Biomass; Individual tree structure; Crown delineation;
Carbon
ID FOREST CARBON STOCKS; ABOVEGROUND BIOMASS; CANOPY STRUCTURE; ALLOMETRIC
EQUATIONS; FOOTPRINT LIDAR; AIRBORNE; HEIGHT; INTEGRATION; TREES; AREA
AB Lidar remote sensing has emerged as one of the best technologies for mapping aboveground biomass in forest systems. Recent developments in lidar instruments, computer processing power, and algorithm development have enabled the mapping of individual tree structure from lidar remote sensing, yet the utility of individual tree metrics has not been fully explored for aboveground biomass mapping. Conversely, scaling-based approaches using minimal data inputs have recently been presented as an alternative method for mapping regional biomass. We compare these two emerging avenues of lidar-based biomass mapping to plot-aggregated biomass modeling techniques. We assess three forested ecosystems: a mature, closed-canopy deciduous broadleaf forest; a mature evergreen needleleaf forest; and a Loblolly pine plantation with a range of even-aged stands. For individual tree based approaches, individual tree metrics improve explanatory power from R-2 = 057 to R-2 = 0.85 in the mature conifer site, but do not show statistically significant improvements in the other two sites. We suggest that with large field sample plots in areas of open canopy cover, individual tree metrics can significantly improve aboveground biomass (AGBM) estimation as they directly take into account stand density. Regarding scalingbased approaches, we demonstrate that the proposed methods are currently unsuitable at local scales in forests without a tight relationship between canopy top height and basal area, as seen in two of our study areas. Individual tree information shows promise for improving AGBM modeling capabilities, and may also facilitate scalingbased approaches, but further research regarding the application of allometric equations and the spatial scale of models is necessary to continue advancing the field of high-resolution forest biomass accounting. (C) 2015 Elsevier Inc All rights reserved.
C1 [Duncanson, L. I.; Dubayah, R. O.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Cook, B. D.; Rosette, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Parker, G.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Duncanson, LI (reprint author), Univ Maryland, Dept Geog Sci, 2181 Lefrak Hall, College Pk, MD 20742 USA.
EM lduncans@umd.edu
OI Parker, Geoffrey/0000-0001-7055-6491
FU NASA Earth and Space Science Fellowship program [016324-001]; Natural
Sciences and Engineering Research Council of Canada (NSERC)'s
Postgraduate Scholarship D3
FX We gratefully acknowledge the NASA Earth and Space Science Fellowship
program (grant number 016324-001), and the Natural Sciences and
Engineering Research Council of Canada (NSERC)'s Postgraduate
Scholarship D3 for funding this work. Thank you to the Smithsonian
Environmental Research Center and SIGEO program for their provision of
SERC field data, and field teams at UMD and GSFC for their field data
collection at Parker Tract and Teakettle. The crown delineation
algorithm was run on the Pleiades supercomputer at NASA Ames through the
NASA Earth Exchange (NEX) program. Additional thanks go to Dr. Anu
Swatantran for the helpful comments on this manuscript and other members
of the Global Ecology Lab. We also gratefully acknowledge the comments
from four anonymous reviewers.
NR 59
TC 9
Z9 9
U1 10
U2 40
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 OCT
PY 2015
VL 168
BP 102
EP 112
DI 10.1016/j.rse.2015.06.021
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CR5SY
UT WOS:000361405500009
ER
PT J
AU Lievens, H
Tomer, SK
Al Bitar, A
De Lannoy, GJM
Drusch, M
Dumedah, G
Franssen, HJH
Kerr, YH
Martens, B
Pan, M
Roundy, JK
Vereecken, H
Walker, JP
Wood, EF
Verhoest, NEC
Pauwels, VRN
AF Lievens, H.
Tomer, S. K.
Al Bitar, A.
De Lannoy, G. J. M.
Drusch, M.
Dumedah, G.
Franssen, H. -J. Hendricks
Kerr, Y. H.
Martens, B.
Pan, M.
Roundy, J. K.
Vereecken, H.
Walker, J. P.
Wood, E. F.
Verhoest, N. E. C.
Pauwels, V. R. N.
TI SMOS soil moisture assimilation for improved hydrologic simulation in
the Murray Darling Basin, Australia
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE SMOS; Data assimilation; Soil moisture; Streamflow; Murray Darling Basin
ID LAND DATA ASSIMILATION; RAINFALL-RUNOFF MODEL; L-BAND; SURFACE MODELS;
DISCHARGE PREDICTIONS; SOUTHEAST AUSTRALIA; RETRIEVAL ALGORITHM; GLOBAL
OPTIMIZATION; MICROWAVE EMISSION; WESTERN DENMARK
AB This study explores the benefits of assimilating SMOS soil moisture retrievals for hydrologic modeling, with a focus on soil moisture and streamflow simulations in the Murray Darling Basin, Australia. In this basin, floods occur relatively frequently and initial catchment storage is known to be key to runoff generation. The land surface model is the Variable Infiltration Capacity (VIC) model. The model is calibrated using the available streamflow records of 169 gauge stations across the Murray Darling Basin. The VIC soil moisture forecast is sequentially updated with observations from the SMOS Level 3 CATDS (Centre Aval de Traitement des Donnees SMOS) soil moisture product using the Ensemble Kalman filter. The assimilation algorithm accounts for the spatial mismatch between the model (0.125) and the SMOS observation (25 km) grids. Three widely-used methods for removing bias between model simulations and satellite observations of soil moisture are evaluated. These methods match the first, second and higher order moments of the soil moisture distributions, respectively. In this study, the first order bias correction, i.e. the rescaling of the long term mean, is the recommended method. Preserving the observational variability of the SMOS soil moisture data leads to improved soil moisture updates, particularly for dry and wet conditions, and enhances initial conditions for runoff generation. Second or higher order bias correction, which includes a rescaling of the variance, decreases the temporal variability of the assimilation results. In comparison with in situ measurements of OzNet the assimilation with mean bias correction reduces the root mean square error (RMSE) of the modeled soil moisture from 0.058 m(3)/m(3) to 0.046 m(3)/m(3) and increases the correlation from 0564 to 0.714. These improvements in antecedent wetness conditions further translate into improved predictions of associated water fluxes, particularly runoff peaks. In conclusion, the results of this study clearly demonstrate the merit of SMOS data assimilation for soil moisture and streamflow predictions at the large scale. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Lievens, H.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium.
[Lievens, H.; Martens, B.; Verhoest, N. E. C.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium.
[Tomer, S. K.; Al Bitar, A.; Kerr, Y. H.] Ctr Etud Spatiales Biosphere, Toulouse, France.
[De Lannoy, G. J. M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Drusch, M.] European Space Agcy, NL-2200 AG Noordwijk, Netherlands.
[Dumedah, G.; Walker, J. P.; Pauwels, V. R. N.] Monash Univ, Dept Civil Engn, Clayton, Vic 3800, Australia.
[Franssen, H. -J. Hendricks; Vereecken, H.] Forschungszentrum Julich, D-52425 Julich, Germany.
[Pan, M.; Wood, E. F.] Princeton Univ, Land Surface Hydrol Grp, Princeton, NJ 08544 USA.
[Roundy, J. K.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
RP Lievens, H (reprint author), Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium.
EM Hans.Lievens@UGent.be
RI Verhoest, Niko/C-9726-2010; Pan, Ming/B-6841-2011; Roundy,
Joshua/H-9377-2016;
OI Verhoest, Niko/0000-0003-4116-8881; Pan, Ming/0000-0003-3350-8719;
Roundy, Joshua/0000-0003-0328-3248; Hendricks-Franssen,
Harrie-Jan/0000-0002-0004-8114; Pauwels, Valentijn/0000-0002-1290-9313;
Martens, Brecht/0000-0002-7368-7953; Al Bitar, Ahmad/0000-0002-1756-1096
FU ESA-STSE project [SR/00/302]; Belgian Science Policy (BELSPO); CNES
Terre, Ocean, Surfaces Continentales, Atmosphere (TOSCA) program;
Australian Research Council
FX The work has been performed in the framework of the ESA-STSE project
'SMOS + Hydrology Study' and was partly funded through project SR/00/302
('Hydras+') financed by the Belgian Science Policy (BELSPO), and the
CNES Terre, Ocean, Surfaces Continentales, Atmosphere (TOSCA) program.
Furthermore, we would like to acknowledge the Australian Bureau of
Meteorology and the University of Melbourne (Andrew Western and
colleagues) for the support in the provision of the streamflow and soil
moisture data. We also would like to acknowledge the Julich
Supercomputing Center for granting computation time on JUROPA. Hans
Lievens is a postdoctoral research fellow of the Research Foundation
Flanders (FWO). Valentijn Pauwels is currently a Future Fellow funded by
the Australian Research Council.
NR 90
TC 18
Z9 18
U1 14
U2 63
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 OCT
PY 2015
VL 168
BP 146
EP 162
DI 10.1016/j.rse.2015.06.025
PG 17
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CR5SY
UT WOS:000361405500013
ER
PT J
AU Long, D
Yang, YT
Wada, Y
Hong, Y
Liang, W
Chen, YN
Yong, B
Hou, AZ
Wei, JF
Chen, L
AF Long, Di
Yang, Yuting
Wada, Yoshihide
Hong, Yang
Liang, Wei
Chen, Yaning
Yong, Bin
Hou, Aizhong
Wei, Jiangfeng
Chen, Lu
TI Deriving scaling factors using a global hydrological model to restore
GRACE total water storage changes for China's Yangtze River Basin
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE GRACE; Scaling factor; PCR-GLOBWB; CLM4.0; GLDAS-1 Noah; Yangtze River;
China
ID LAND-SURFACE MODEL; GROUNDWATER DEPLETION; WELL OBSERVATIONS; ENERGY
FLUXES; SOIL-MOISTURE; MIDDLE-EAST; EVAPOTRANSPIRATION; TEMPERATURE;
SATELLITES; BALANCE
AB This study used a global hydrological model (GHM), PCR-GLOBWB, which simulates surface water storage changes, natural and human induced groundwater storage changes, and the interactions between surface water and subsurface water, to generate scaling factors by mimicking low-pass filtering of GRACE signals. Signal losses in GRACE data were subsequently restored by the scaling factors from PCR-GLOBWB. Results indicate greater spatial heterogeneity in scaling factor from PCR-GLOBWB and CLM4.0 than that from GLDAS-1 Noah due to comprehensive simulation of surface and subsurface water storage changes for PCR-GLOBWB and CLM4.0. Filtered GRACE total water storage (TWS) changes applied with PCR-GLOBWB scaling factors show closer agreement with water budget estimates of TWS changes than those with scaling factors from other land surface models (LSMs) in China's Yangtze River basin. Results of this study develop a further understanding of the behavior of scaling factors from different LSMs or GHMs over hydrologically complex basins, and could be valuable in providing more accurate TWS changes for hydrological applications (e.g., monitoring drought and groundwater storage depletion) over regions where human-induced interactions between surface water and subsurface water are intensive. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Long, Di; Hong, Yang] Tsinghua Univ, Dept Hydraul Engn, State Key Lab Hydrosci & Engn, Beijing 100084, Peoples R China.
[Yang, Yuting] CSIRO Land & Water, Canberra, ACT 2601, Australia.
[Wada, Yoshihide] Univ Utrecht, Dept Phys Geog, Utrecht, Netherlands.
[Wada, Yoshihide] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Wada, Yoshihide] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Hong, Yang] Univ Oklahoma, Dept Civil Engn & Environm Sci, Norman, OK 73019 USA.
[Liang, Wei] Shaanxi Normal Univ, Dept Tourism & Environm Sci, Xian 710119, Shaanxi, Peoples R China.
[Chen, Yaning] Chinese Acad Sci, Xinjiang Inst Ecol & Geog, State Key Lab Desert & Oasis Ecol, Urumqi 830011, Xinjiang, Peoples R China.
[Yong, Bin] Hohai Univ, State Key Lab Hydrol Water Resources & Hydraul En, Nanjing 210098, Jiangsu, Peoples R China.
[Hou, Aizhong] Minist Water Resources, Bur Hydrol, Beijing 100053, Peoples R China.
[Wei, Jiangfeng] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA.
[Chen, Lu] Huazhong Univ Sci & Technol, Coll Hydropower & Informat Engn, Wuhan 430074, Hubei, Peoples R China.
RP Long, D (reprint author), Tsinghua Univ, Dept Hydraul Engn, State Key Lab Hydrosci & Engn, Beijing 100084, Peoples R China.
EM dlong@tsinghua.edu.cn
RI Wada, Yoshihide/F-3595-2012; Long, Di/N-8049-2013; yang,
yuting/C-8527-2014; Wei, Jiangfeng/C-6342-2009; Hong, Yang/D-5132-2009;
Yong, Bin/C-2257-2014
OI Wada, Yoshihide/0000-0003-4770-2539; Long, Di/0000-0001-9033-5039; yang,
yuting/0000-0002-4573-1929; Wei, Jiangfeng/0000-0001-8981-8674; Hong,
Yang/0000-0001-8720-242X; Yong, Bin/0000-0003-1466-2091
FU National Science Foundation of China Major Research Programs [91437214,
71461010701]; Open Research Fund Program of the State Key Laboratory of
Hydroscience and Engineering at Tsinghua University [sklhse-2014-A-02,
sklhse-2014-A-01]
FX This study was jointly supported by the National Science Foundation of
China Major Research Programs (No. 91437214 and No. 71461010701), and
the Open Research Fund Program of the State Key Laboratory of
Hydroscience and Engineering at Tsinghua University (Grant No.
sklhse-2014-A-02 and sklhse-2014-A-01). We thank Dr. Laurent
Longuevergne with Universite de Rennes in France for helping with
learning forward modeling techniques. We are grateful to editors and
four reviewers for their valuable comments and constructive suggestions.
This paper has been greatly improved as a result of their efforts.
NR 85
TC 22
Z9 22
U1 15
U2 50
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 OCT
PY 2015
VL 168
BP 177
EP 193
DI 10.1016/j.rse.2015.07.003
PG 17
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CR5SY
UT WOS:000361405500015
ER
PT J
AU Mackey, J
Dynys, F
Sehirliogiu, A
AF Mackey, Jon
Dynys, Frederick
Sehirliogiu, Alp
TI Si/Ge-WSi2 composites: Processing and thermoelectric properties
SO ACTA MATERIALIA
LA English
DT Article
DE Thermoelectric materials; Seebeck coefficient; Electrical resistivity;
Thermal conductivity; Nano-structure
ID SILICON-GERMANIUM ALLOY; TRANSPORT-PROPERTIES; HEAT-CAPACITY;
THIN-FILMS; PRECIPITATION; CONDUCTIVITY; SI
AB Thermoelectric nano-composites composed of a Si/Ge matrix with WSi2 nano-precipitates were investigated and reductions in lattice thermal conductivity as large as 40% (compared to a benchmark suicide free sample) have been achieved. Additionally, samples exhibited enhanced figure of merit over that of classic state-of-the art Si/Ge, improvements as large as 30% were obtained for both p-type and n-type samples. Samples were prepared from powder metallurgic techniques; mechano-chemical alloying in a planetary mill combined with spark plasma sintering for densification. Thermoelectric properties and microstructure of the specimens were investigated in relationship to processing conditions and composition. The nano-composites investigated in this work provide both a viable enhancement mechanism with greater thermal stability and an experimental benchmark for theoretic work on silicide inclusions in Si/Ge matrix. This experimental work verifies the prospect to enhance figure of merit, and demonstrates that achieving uniform WSi2 nano-inclusion is a technical challenge using powder processing approach. (C) 2015 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Mackey, Jon] Univ Akron, Mech Engn, Akron, OH 44325 USA.
[Dynys, Frederick] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Sehirliogiu, Alp] Case Western Reserve Univ, Mat Sci & Engn, Cleveland, OH 44106 USA.
RP Mackey, J (reprint author), Univ Akron, Mech Engn, Akron, OH 44325 USA.
EM jam151@zips.uakron.edu; Frederick.w.dynys@nasa.gov; axs461@case.edu
FU NASA/USRA [04555-004]; NASA Radioisotope Power System program
FX The authors would like to thank Ben Kowalski, Serene Farmer, Tom Sabo,
and Ray Babuder from NASA Glenn Research Center and Case Western Reserve
University as well as Sabah Bux and Jean-Pierre Fleurial from NASA JPL
for their assistance and insightful conversations. The STEM work was
performed by Elahe Farghadany from Case Western Reserve University. The
spark plasma sintering equipment used in this work was generously
provided by Mike Cinibulk from the Air Force Research Laboratories at
Wright-Patterson Air Force Base. The authors also gratefully acknowledge
funding source NASA/USRA 04555-004 and the NASA Radioisotope Power
System program.
NR 35
TC 2
Z9 2
U1 1
U2 19
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6454
EI 1873-2453
J9 ACTA MATER
JI Acta Mater.
PD OCT 1
PY 2015
VL 98
BP 263
EP 274
DI 10.1016/j.actamat.2015.07.025
PG 12
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA CR1GX
UT WOS:000361074000026
ER
PT J
AU Hernandez-Stefanoni, JL
Johnson, KD
Cook, BD
Dupuy, JM
Birdsey, R
Peduzzi, A
Tun-Dzul, F
AF Luis Hernandez-Stefanoni, Jose
Johnson, Kristofer D.
Cook, Bruce D.
Manuel Dupuy, Juan
Birdsey, Richard
Peduzzi, Alicia
Tun-Dzul, Fernando
TI Estimating species richness and biomass of tropical dry forests using
LIDAR during leaf-on and leaf-off canopy conditions
SO APPLIED VEGETATION SCIENCE
LA English
DT Article
DE Above-ground biomass; Canopy conditions; Forest structure; Species
richness; LIDAR; Topography; Tropical dry forest
ID AIRBORNE LIDAR; YUCATAN PENINSULA; ALPHA-DIVERSITY; SCALE VARIATION;
REGIONAL-SCALE; TREE HEIGHT; CARBON; MEXICO; DENSITY; SLOPE
AB QuestionsIs the accuracy of predictions of above-ground biomass (AGB) and plant species richness of tropical dry forests from LIDAR data compromised during leaf-off canopy period, when most of the vegetation is leafless, compared to the leaf-on period? How does topographic position affect prediction accuracy of AGB for leaf-off and leaf-on canopy conditions?
LocationTropical dry forest, Yucatan Peninsula, Mexico.
MethodsWe evaluated the accuracy of predictions using both leaf-on and leaf-off LIDAR estimates of biomass and species richness, and assessed the adequacy of both LIDAR data sets for characterizing these vegetation attributes in tropical dry forests using multiple regression analysis and ANOVA. The performance of the models was assessed by leave-one-out cross-validation. We also investigated differences in vegetation structure between two topographic conditions using PCA and ANOSIM. Finally, we evaluated the influence of topography on the accuracy of biomass estimates from LIDAR using multiple regression analysis and ANOVA.
ResultsA higher overall accuracy was obtained with leaf-on vs leaf-off conditions for AGB (root mean square error (RMSE)=21.6 vs 25.7tonha(-1)), as well as for species richness (RMSE=5.5 vs 5.8 species, respectively). However, no significant differences in mean dissimilarities between biomass estimates from LIDAR and in situ biomass estimates comparing the two canopy conditions were found (F-1,F-39=0.03, P=0.87). In addition, no significant differences in dissimilarities of AGB estimation were found between flat and hilly areas (F-1,F-39=1.36, P=0.25).
ConclusionsOur results suggest that estimates of species richness and AGB from LIDAR are not significantly influenced by canopy conditions or slope, indicating that both leaf-on and leaf-off models are appropriate for these variables regardless of topographic position in these tropical dry forests.
C1 [Luis Hernandez-Stefanoni, Jose; Manuel Dupuy, Juan; Tun-Dzul, Fernando] Ctr Invest Cient Yucatan AC, Unidad Recursos Nat, Merida 97200, Yucatan, Mexico.
[Johnson, Kristofer D.; Birdsey, Richard; Peduzzi, Alicia] US Forest Serv, No Res Stn, Newtown Sq, PA 19073 USA.
[Cook, Bruce D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hernandez-Stefanoni, JL (reprint author), Ctr Invest Cient Yucatan AC, Unidad Recursos Nat, Calle 43 130, Merida 97200, Yucatan, Mexico.
EM jl_stefanoni@cicy.mx; kristoferdjohnson@fs.fed.us; bruce.cook@nasa.gov;
jmdupuy@cicy.mx; rbirdsey@fs.fed.us; apeduzzi@fs.fed.us; fjtun@cicy.mx
FU Reinforcing REDD+ and South-South Cooperation Project - Mexican National
Forest Commission (CONAFOR); United States Forest Service (USFS); USAID
FX We are grateful to Kaxil Kiuic A. C. for logistic support, and Filogonio
May-Pat and Manuela Tamayo for assistance with fieldwork and data
processing. We also thank two anonymous reviewers and the editor, whose
constructive and insightful comments helped improve the clarity and
impact of this paper. The study was financially supported by the
Reinforcing REDD+ and South-South Cooperation Project, funded by the
Mexican National Forest Commission (CONAFOR), United States Forest
Service (USFS) and USAID. This study is part of the Mexican network of
Intensive Carbon Monitoring Sites (MEX-SMIC), an affiliation of academic
institutions, government and NGOs with various funding sources. The
network currently includes five forested sites located in strategic
landscapes for REDD+ activities in Mexico.
NR 48
TC 2
Z9 2
U1 7
U2 38
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1402-2001
EI 1654-109X
J9 APPL VEG SCI
JI Appl. Veg. Sci.
PD OCT
PY 2015
VL 18
IS 4
BP 724
EP 732
DI 10.1111/avsc.12190
PG 9
WC Plant Sciences; Ecology; Forestry
SC Plant Sciences; Environmental Sciences & Ecology; Forestry
GA CR2SU
UT WOS:000361181500018
ER
PT J
AU Straume, T
Braby, LA
Borak, TB
Lusby, T
Warner, DW
Perez-Nunez, D
AF Straume, T.
Braby, L. A.
Borak, T. B.
Lusby, T.
Warner, D. W.
Perez-Nunez, D.
TI Compact Tissue-equivalent Proportional Counter for Deep Space Human
Missions
SO HEALTH PHYSICS
LA English
DT Article
ID VARIANCE-COVARIANCE METHOD; RADIATION-FIELDS; PARTICLES; ENERGY
AB Effects on human health from the complex radiation environment in deep space have not been measured and can only be simulated here on Earth using experimental systems and beams of radiations produced by accelerators, usually one beam at a time. This makes it particularly important to develop instruments that can be used on deep-space missions to measure quantities that are known to be relatable to the biological effectiveness of space radiation. Tissue-equivalent proportional counters (TEPCs) are such instruments. Unfortunately, present TEPCs are too large and power intensive to be used beyond low Earth orbit (LEO). Here, the authors describe a prototype of a compact TEPC designed for deep space applications with the capability to detect both ambient galactic cosmic rays and intense solar particle event radiation. The device employs an approach that permits real-time determination of
[GRAPHICS]
(and thus quality factor) using a single detector. This was accomplished by assigning sequential sampling intervals as detectors "1" and "2" and requiring the intervals to be brief compared to the change in dose rate. Tests with gamma rays show that the prototype instrument maintains linear response over the wide dose-rate range expected in space with an accuracy of better than 5% for dose rates above 3 mGy h(-1). Measurements of
[GRAPHICS]
for 200 MeV n(-1) carbon ions were better than 10%. Limited tests with fission spectrum neutrons show absorbed dose-rate accuracy better than 15%.
C1 [Straume, T.; Lusby, T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Braby, L. A.; Perez-Nunez, D.] Texas A&M Univ, College Stn, TX 77843 USA.
[Borak, T. B.; Warner, D. W.] Colorado State Univ, Ft Collins, CO 80523 USA.
RP Straume, T (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Tore.Straume-1@nasa.gov
FU National Space Biomedical Research Institute (NSBRI) through NASA Ames
Research Center [RE01302]; Texas AM University; Colorado State
University [RE01301]
FX The authors acknowledge support from the National Space Biomedical
Research Institute (NSBRI) through grant RE01302 at NASA Ames Research
Center (T. Straume, PI) and Texas A&M University (L. Braby, Co-PI), and
grant RE01301 at Colorado State University (T. Borak, PI). We wish to
acknowledge the support and assistance provided by administrative and
technical personnel at the Heavy Ion Medical Accelerator (HIMAC) at the
National Institute of Radiological Sciences in Chiba, Japan; at the NASA
Space Radiation Laboratory (NSRL) in Brookhaven National Laboratory; at
the 88" Cyclotron Facility at the Lawrence Berkeley National Laboratory;
and at the Stanford Linear Accelerator Center (SLAC). Valuable advice
and assistance were provided by C. Zeitlin and K. Neal at the Southwest
Research Institute (SwRI) and J. Miller at LBNL. Graduate students L.
Manglass and D. Oertli were instrumental in assembling equipment,
performing experiments and analyzing data at Colorado State University
(CSU). R. Adame and J. Jablonski (CSU) were responsible for timely and
precise manufacturing of parts and supplies for detector components. H.
Tran was responsible for microelectronics and microprocessor programming
support at NASA Ames and H. Liu supported the pre-amplifier development
efforts at TAMU.
NR 16
TC 1
Z9 1
U1 2
U2 5
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA
SN 0017-9078
EI 1538-5159
J9 HEALTH PHYS
JI Health Phys.
PD OCT
PY 2015
VL 109
IS 4
BP 277
EP 283
DI 10.1097/HP.0000000000000334
PG 7
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA CQ8DT
UT WOS:000360837200002
PM 26313585
ER
PT J
AU Viola, M
Cacciato, M
Brouwer, M
Kuijken, K
Hoekstra, H
Norberg, P
Robotham, ASG
van Uitert, E
Alpaslan, M
Baldry, IK
Choi, A
de Jong, JTA
Driver, SP
Erben, T
Grado, A
Graham, AW
Heymans, C
Hildebrandt, H
Hopkins, AM
Irisarri, N
Joachimi, B
Loveday, J
Miller, L
Nakajima, R
Schneider, P
Sifon, C
Kleijn, GV
AF Viola, M.
Cacciato, M.
Brouwer, M.
Kuijken, K.
Hoekstra, H.
Norberg, P.
Robotham, A. S. G.
van Uitert, E.
Alpaslan, M.
Baldry, I. K.
Choi, A.
de Jong, J. T. A.
Driver, S. P.
Erben, T.
Grado, A.
Graham, Alister W.
Heymans, C.
Hildebrandt, H.
Hopkins, A. M.
Irisarri, N.
Joachimi, B.
Loveday, J.
Miller, L.
Nakajima, R.
Schneider, P.
Sifon, C.
Kleijn, G. Verdoes
TI Dark matter halo properties of GAMA galaxy groups from 100 square
degrees of KiDS weak lensing data
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: observational; methods: statistical; galaxies: groups: general;
galaxies: haloes; dark matter; large-scale structure of Universe
ID MASS ASSEMBLY GAMA; DIGITAL SKY SURVEY; LARGE-SCALE BIAS; TO-LIGHT
RATIOS; X-RAY; STELLAR MASS; REDSHIFT SURVEY; COSMOLOGICAL CONSTRAINTS;
SATELLITE KINEMATICS; LUMINOSITY-RELATION
AB The Kilo-Degree Survey is an optical wide-field survey designed to map the matter distribution in the Universe using weak gravitational lensing. In this paper, we use these data to measure the density profiles and masses of a sample of similar to 1400 spectroscopically identified galaxy groups and clusters from the Galaxy And Mass Assembly survey. We detect a highly significant signal (signal-to-noise-ratio similar to 120), allowing us to study the properties of dark matter haloes over one and a half order of magnitude in mass, from M similar to 10(13)-10(14.5) h(-1) M-circle dot. We interpret the results for various subsamples of groups using a halo model framework which accounts for the mis-centring of the brightest cluster galaxy (used as the tracer of the group centre) with respect to the centre of the group's dark matter halo. We find that the density profiles of the haloes are well described by an NFW profile with concentrations that agree with predictions from numerical simulations. In addition, we constrain scaling relations between the mass and a number of observable group properties. We find that the mass scales with the total r-band luminosity as a power law with slope 1.16 +/- 0.13 (1 sigma) and with the group velocity dispersion as a power law with slope 1.89 +/- 0.27 (1 sigma). Finally, we demonstrate the potential of weak lensing studies of groups to discriminate between models of baryonic feedback at group scales by comparing our results with the predictions from the Cosmo-OverWhelmingly Large Simulations project, ruling out models without AGN feedback.
C1 [Viola, M.; Cacciato, M.; Brouwer, M.; Kuijken, K.; Hoekstra, H.; de Jong, J. T. A.; Irisarri, N.; Sifon, C.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Norberg, P.] Univ Durham, Dept Phys, ICC, Durham DH1 3LE, England.
[Robotham, A. S. G.; Driver, S. P.] Univ Western Australia, Sch Phys, ICRAR, Crawley, WA 6009, Australia.
[van Uitert, E.; Joachimi, B.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[van Uitert, E.; Erben, T.; Hildebrandt, H.; Nakajima, R.; Schneider, P.] Argelander Inst Astron, D-53121 Bonn, Germany.
[Alpaslan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Baldry, I. K.] Liverpool John Moores Univ, Astrophys Res Inst, IC2, Liverpool L3 5RF, Merseyside, England.
[Choi, A.; Heymans, C.] Univ Edinburgh, Royal Observ, Inst Astron, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Driver, S. P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Grado, A.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Graham, Alister W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Hopkins, A. M.] Australian Astron Observ, N Ryde, NSW 1670, Australia.
[Loveday, J.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Miller, L.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Kleijn, G. Verdoes] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
RP Viola, M (reprint author), Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
EM viola@strw.leidenuniv.nl
OI Grado, Aniello/0000-0002-0501-8256; Robotham, Aaron/0000-0003-0429-3579;
Alpaslan, Mehmet/0000-0003-0321-1033; Sifon,
Cristobal/0000-0002-8149-1352; Baldry, Ivan/0000-0003-0719-9385
FU European Research Council [279396, 240185, DEGAS-259586]; STFC
[ST/J004421/1, ST/L00285X/1]; Royal Society; Science and Technology
Facilities Council [ST/L00075X/1]; German Federal Ministry for Economic
Affairs and Energy (BMWi) provided via DLR [50QE1103]; DFG Emmy Noether
grant [Hi 1495/2-1]; Netherlands Organization for Scientific Research
(NWO) [614.001.103, 614.061.610]; Deutsche Forschungsgemeinschaft
[TR33]; ESO Telescopes at the La Silla Paranal Observatory [177.A-3016,
177.A-3017, 177.A-3018]; STFC (UK); ARC (Australia); AAO
FX We would like to thank the anonymous referee for providing useful
suggestions to improve the manuscript. We thank Tom Kitching, Joachim
Harnois-Deraps, Martin Eriksen and Mario Radovich for providing useful
comments to the paper. We are grateful to Matthias Bartelmann for being
our external blinder, revealing which of the four catalogues analysed
was the true unblinded catalogue at the end of this study. We would like
to thank Tamsyn Mcnaught-Roberts for providing the conversion between
the halo mass definition used in the GAMA mocks and M200, and
Ian McCarthy for providing the data used in Fig. 15. We also thank Ludo
van Waerbeke for writing the code used to compute the shear additive
bias correction used in this work. MV, MC, HHo, CS, AC, and CH
acknowledge support from the European Research Council under FP7 grant
number 279396 (MV, MC, CS, H.Ho) and 240185 (AC and CH). BJ acknowledges
support by an STFC Ernest Rutherford Fellowship, grant reference
ST/J004421/1. EvU acknowledges support from an STFC Ernest Rutherford
Research Grant, grant reference ST/L00285X/1. PN acknowledges the
support of the Royal Society through the award of a University Research
Fellowship, the European Research Council, through receipt of a Starting
Grant (DEGAS-259586) and support of the Science and Technology
Facilities Council (ST/L00075X/1). RN and EvU acknowledge support from
the German Federal Ministry for Economic Affairs and Energy (BMWi)
provided via DLR under project no. 50QE1103. HHi is supported by the DFG
Emmy Noether grant Hi 1495/2-1. This work is supported by the
Netherlands Organization for Scientific Research (NWO) through grants
614.001.103 (MV) and 614.061.610 (JdJ) and by the Deutsche
Forschungsgemeinschaft in the framework of the TR33 'The Dark Universe'.
This work is based on data products from observations made with ESO
Telescopes at the La Silla Paranal Observatory under programme IDs
177.A-3016, 177.A-3017, and 177.A-3018. GAMA is a joint
European-Australasian project based around a spectroscopic campaign
using the Anglo-Australian Telescope. The GAMA input catalogue is based
on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared
Deep Sky Survey. Complementary imaging of the GAMA regions is being
obtained by a number of independent survey programs including GALEX MIS,
VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing
UV to radio coverage. GAMA is funded by the STFC (UK), the ARC
(Australia), the AAO, and the participating institutions. The GAMA
website is http://www.gama-survey.org/.
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 1
PY 2015
VL 452
IS 4
BP 3529
EP 3550
DI 10.1093/mnras/stv1447
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8MO
UT WOS:000360862100019
ER
PT J
AU LaCourse, DM
Jek, KJ
Jacobs, TL
Winarski, T
Boyajian, TS
Rappaport, SA
Sanchis-Ojeda, R
Conroy, KE
Nelson, L
Barclay, T
Fischer, DA
Schmitt, JR
Wang, J
Stassun, KG
Pepper, J
Coughlin, JL
Shporer, A
Prsa, A
AF LaCourse, Daryll M.
Jek, Kian J.
Jacobs, Thomas L.
Winarski, Troy
Boyajian, Tabetha S.
Rappaport, Saul A.
Sanchis-Ojeda, Roberto
Conroy, Kyle E.
Nelson, Lorne
Barclay, Tom
Fischer, Debra A.
Schmitt, Joseph R.
Wang, Ji
Stassun, Keivan G.
Pepper, Joshua
Coughlin, Jeffrey L.
Shporer, Avi
Prsa, Andrej
TI Kepler eclipsing binary stars - VI. Identification of eclipsing binaries
in the K2 Campaign 0 data set
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: photometric; binaries: eclipsing; stars: fundamental
parameters; stars: general; planetary systems; stars: statistics
ID PLANET CANDIDATES; MAIN-SEQUENCE; LIGHT CURVES; DATA RELEASE; ARCHIVE
DATA; PHOTOMETRY; MISSION; FIELD; CATALOG; SYSTEM
AB The original Kepler mission observed and characterized over 2400 eclipsing binaries (EBs) in addition to its prolific exoplanet detections. Despite the mechanical malfunction and subsequent non-recovery of two reaction wheels used to stabilize the instrument, the Kepler satellite continues collecting data in its repurposed K2 mission surveying a series of fields along the ecliptic plane. Here, we present an analysis of the first full baseline K2 data release: the Campaign 0 data set. In the 7761 light curves we have identified a total of 207 EBs. Of these, 97 are new discoveries that were not previously identified. Our pixel-level analysis of these objects has also resulted in identification of several false positives (observed targets contaminated by neighbouring EBs), as well as the serendipitous discovery of two short-period exoplanet candidates. We provide catalogue cross-matched source identifications, orbital periods, morphologies and ephemerides for these eclipsing systems. We also describe the incorporation of the K2 sample into the Kepler Eclipsing Binary Catalog, present spectroscopic follow-up observations for a limited selection of nine systems and discuss prospects for upcoming K2 campaigns.
C1 [Boyajian, Tabetha S.; Fischer, Debra A.; Schmitt, Joseph R.; Wang, Ji] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Rappaport, Saul A.; Sanchis-Ojeda, Roberto] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Rappaport, Saul A.; Sanchis-Ojeda, Roberto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Conroy, Kyle E.; Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, VU Stn B 1807, Nashville, TN 37235 USA.
[Nelson, Lorne] Bishops Univ, Dept Phys, Sherbrooke, PQ J1M 1Z7, Canada.
[Barclay, Tom] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
[Pepper, Joshua] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA.
[Coughlin, Jeffrey L.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Prsa, Andrej] Villanova Univ, Dept Astrophys & Planetary Sci, Villanova, PA 19085 USA.
EM daryll.lacourse@gmail.com; tabetha.boyajian@yale.edu
OI Schmitt, Joseph/0000-0003-1874-0552; Pepper, Joshua/0000-0002-3827-8417
FU NASAs Science Mission Directorate; NASA [ADAP12-0172, ADAP14-0245];
Natural Sciences and Engineering Research Council (NSERC) of Canada;
NASA Office of Space Science [NNX13AC07G]; National Aeronautics and
Space Administration; Space Telescope Science Institute under U.S.
Government [NAG W-2166]; Association of Universities for Research in
Astronomy, Inc., under NASA [NAS5-26555]; National Science Foundation
FX Funding for the Kepler and K2 Discovery missions is provided by NASAs
Science Mission Directorate. TSB, DAF, JW and JRS acknowledge support
provided through NASA grant ADAP12-0172 and ADAP14-0245. LN thanks the
Natural Sciences and Engineering Research Council (NSERC) of Canada for
financial support, and the staff at the Observatoire Astronomique du
Mont-Megantic for their technical assistance. 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. 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 the VizieR catalogue
access tool, CDS, Strasbourg, France. The original description of the
VizieR service was published in Ochsenbein, Bauer & Marcout (2000). This
research has made use of the SIMBAD data base, operated at CDS,
Strasbourg, France (Wenger et al. 2000). This research has made use of
the VSX data base, operated at AAVSO, Cambridge, Massachusetts, USA.
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 publication makes use of data
products from the Wide-field Infrared Survey Explorer, which is a joint
project of the University of California, Los Angeles, and the Jet
Propulsion Laboratory/California Institute of Technology, funded by the
National Aeronautics and Space Administration. The Digitized Sky Surveys
were produced at the Space Telescope Science Institute under U.S.
Government grant NAG W-2166. The images of these surveys are based on
photographic data obtained using the Oschin Schmidt Telescope on Palomar
Mountain and the UK Schmidt Telescope. The plates were processed into
the present compressed digital form with the permission of these
institutions.
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EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 1
PY 2015
VL 452
IS 4
BP 3561
EP 3592
DI 10.1093/mnras/stv1475
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8MO
UT WOS:000360862100021
ER
PT J
AU Rawlings, JI
Page, MJ
Symeonidis, M
Bock, J
Cooray, A
Farrah, D
Guo, K
Hatziminaoglou, E
Ibar, E
Oliver, SJ
Roseboom, IG
Scott, D
Seymour, N
Vaccari, M
Wardlow, JL
AF Rawlings, J. I.
Page, M. J.
Symeonidis, M.
Bock, J.
Cooray, A.
Farrah, D.
Guo, K.
Hatziminaoglou, E.
Ibar, E.
Oliver, S. J.
Roseboom, I. G.
Scott, Douglas
Seymour, N.
Vaccari, M.
Wardlow, J. L.
TI HerMES: disentangling active galactic nuclei and star formation in the
radio source population
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: ISM-galaxies: nuclei; infrared: galaxies;
radio continuum: galaxies
ID DEEP FIELD-SOUTH; SPECTRAL ENERGY-DISTRIBUTIONS; SPITZER MIDINFRARED
SPECTROSCOPY; INFRARED LUMINOUS GALAXIES; MS SOURCE CATALOGS; YALE-CHILE
MUSYC; 1.4 GHZ SURVEY; HIGH-REDSHIFT; EXTRAGALACTIC SURVEY;
HERSCHEL-SPIRE
AB We separate the extragalactic radio source population above similar to 50 mu Jy into active galactic nuclei (AGN) and star-forming sources. The primary method of our approach is to fit the infrared spectral energy distributions (SEDs), constructed using Spitzer/IRAC (Infrared Array Camera) and Multiband Imaging Photometer for Spitzer (MIPS) and Herschel/SPIRE photometry, of 380 radio sources in the Extended Chandra Deep Field-South. From the fitted SEDs, we determine the relative AGN and star-forming contributions to their infrared emission. With the inclusion of other AGN diagnostics such as X-ray luminosity, Spitzer/IRAC colours, radio spectral index and the ratio of star-forming total infrared flux to k-corrected 1.4 GHz flux density, qIR, we determine whether the radio emission in these sources is powered by star formation or by an AGN. The majority of these radio sources (60 per cent) show the signature of an AGN at some wavelength. Of the sources with AGN signatures, 58 per cent are hybrid systems for which the radio emission is being powered by star formation. This implies that radio sources which have likely been selected on their star formation have a high AGN fraction. Below a 1.4 GHz flux density of 1 mJy, along with finding a strong contribution to the source counts from pure star-forming sources, we find that hybrid sources constitute 20-65 per cent of the sources. This result suggests that hybrid sources have a significant contribution, along with sources that do not host a detectable AGN, to the observed flattening of the source counts at similar to 1 mJy for the extragalactic radio source population.
C1 [Rawlings, J. I.; Page, M. J.; Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Symeonidis, M.; Guo, K.; Oliver, S. J.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Bock, J.] CALTECH, Pasadena, CA 91125 USA.
[Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Hatziminaoglou, E.] ESO, D-85748 Garching, Germany.
[Ibar, E.] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile.
[Roseboom, I. G.] Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Seymour, N.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa.
[Vaccari, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy.
[Wardlow, J. L.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
RP Rawlings, JI (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
EM jason.rawlings.09@ucl.ac.uk
RI Vaccari, Mattia/R-3431-2016; Wardlow, Julie/C-9903-2015;
OI Vaccari, Mattia/0000-0002-6748-0577; Wardlow, Julie/0000-0003-2376-8971;
Scott, Douglas/0000-0002-6878-9840; Seymour,
Nicholas/0000-0003-3506-5536
FU Science and Technologies Facilities Council studentship; Science and
Technology Facilities Council (STFC) [ST/K000977/1]; STFC
[ST/I000976/1]; Australian Research Council Future Fellowship; South
African Department of Science and Technology [DST/CON 0134/2014];
European Commission Research Executive Agency [FP7-SPACE-2013-1 GA
607254]; Italian Ministry for Foreign Affairs and International
Cooperation [PGR GA ZA14GR02]; Danish National Research Foundation; CSA
(Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI
(Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA)
FX We thank the anonymous referee for their comments which improved the
manuscript. We also thank Neal Miller for useful discussions and James
Mullaney for help regarding DecompIR. JIR acknowledges the support of a
Science and Technologies Facilities Council studentship. MJP
acknowledges support from the Science and Technology Facilities Council
(STFC) (grant number ST/K000977/1). SJO and MS acknowledge support from
the STFC (grant number ST/I000976/1). NS is the recipient of an
Australian Research Council Future Fellowship. MV acknowledges support
from the South African Department of Science and Technology (DST/CON
0134/2014), the European Commission Research Executive Agency
(FP7-SPACE-2013-1 GA 607254) and the Italian Ministry for Foreign
Affairs and International Cooperation (PGR GA ZA14GR02). The Dark
Cosmology Centre is funded by the Danish National Research Foundation.
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 (UK); and NASA (USA). This work is also
based on observations made with the Spitzer Space Telescope, which is
operated by the Jet Propulsion Laboratory (JPL), California Institute of
Technology (Caltech) under contract with NASA. This work benefitted from
the NASA/IPAC Extragalactic Database (NED), which is operated by the
JPL, Caltech, under contract with NASA.
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PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
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JI Mon. Not. Roy. Astron. Soc.
PD OCT 1
PY 2015
VL 452
IS 4
BP 4111
EP 4127
DI 10.1093/mnras/stv1573
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8MO
UT WOS:000360862100057
ER
PT J
AU Brown, GC
Levan, AJ
Stanway, ER
Tanvir, NR
Cenko, SB
Berger, E
Chornock, R
Cucchiaria, A
AF Brown, G. C.
Levan, A. J.
Stanway, E. R.
Tanvir, N. R.
Cenko, S. B.
Berger, E.
Chornock, R.
Cucchiaria, A.
TI Swift J1112.2-8238: a candidate relativistic tidal disruption flare
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: nuclei; gamma-rays: galaxies
ID GAMMA-RAY BURST; SUPERMASSIVE BLACK-HOLES; RADIO IMAGING SURVEY; DIGITAL
SKY SURVEY; X-RAY; STAR-FORMATION; OPTICAL AFTERGLOWS; GALACTIC NUCLEI;
SOURCE CATALOG; SOUTHERN SKY
AB We present observations of Swift J1112.2-8238, and identify it as a candidate relativistic tidal disruption flare. The outburst was first detected by Swift/Burst Alert Telescope (BAT) in 2011 June as an unknown, long-lived (order of days) gamma-ray transient source. We show that its position is consistent with the nucleus of a faint galaxy for which we establish a likely redshift of z = 0.89 based on a single emission line that we interpret as the blended [O II] lambda 3727 doublet. At this redshift, the peak X-ray/gamma-ray luminosity exceeded 10(47) erg s(-1), while a spatially coincident optical transient source had i' similar to 22 (M-g similar to -21.4 at z = 0.89) during early observations, similar to 20 d after the Swift trigger. These properties place Swift J1112.2-8238 in a very similar region of parameter space to the two previously identified members of this class, Swift J1644+57 and Swift J2058+0516. As with those events the high-energy emission shows evidence for variability over the first few days, while late-time observations, almost 3 yr post-outburst, demonstrate that it has now switched off. Swift J1112.2-8238 brings the total number of such events observed by Swift to three, interestingly all detected by Swift over a similar to 3 month period (<3 per cent of its total lifetime as of 2015 March). While this suggests the possibility that further examples may be uncovered by detailed searches of the BAT archives, the lack of any prime candidates in the years since 2011 means these events are undoubtedly rare.
C1 [Brown, G. C.; Levan, A. J.; Stanway, E. R.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Cenko, S. B.; Cucchiaria, A.] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chornock, R.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
RP Brown, GC (reprint author), Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England.
EM g.c.brown@warwick.ac.uk
OI Stanway, Elizabeth/0000-0002-8770-809X
FU STFC [ID ST/I001719/1]; Leverhulme Trust via a Philip Leverhulme Prize;
ESO Telescopes at the La Silla Paranal Observatory [089.B-0860]
FX We thank the referee for a careful and thoughtful report that has
improved this paper. GCB thanks the Midlands Physics Alliance for a PhD
studentship. AJL thanks STFC for support under grant ID ST/I001719/1,
and the Leverhulme Trust for support via a Philip Leverhulme Prize.
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). Based on observations made with ESO Telescopes
at the La Silla Paranal Observatory under programme ID 089.B-0860. We
have made use of the ROSAT Data Archive of the Max-Planck-Institut fr
extraterrestrische Physik (MPE) at Garching, Germany. Swift/BAT
transient monitor results provided by the Swift/BAT team. This work made
use of data supplied by the UK Swift Science Data Centre at the
University of Leicester.
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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 OCT 1
PY 2015
VL 452
IS 4
BP 4297
EP 4306
DI 10.1093/mnras/stv1520
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8MO
UT WOS:000360862100072
ER
PT J
AU Bonneville, A
Heggy, E
Strickland, C
Normand, J
Dermond, J
Fang, YL
Sullivan, C
AF Bonneville, Alain
Heggy, Essam
Strickland, Christopher
Normand, Jonathan
Dermond, Jeffrey
Fang, Yilin
Sullivan, Charlotte
TI Geophysical Monitoring of Ground Surface Deformation Associated with a
Confined Aquifer Storage and Recovery Operation
SO WATER RESOURCES MANAGEMENT
LA English
DT Article
DE Water storage; CO2 storage; Ground deformation; INSAR; GPS; Gravity;
ASR; Aquifer storage and recovery
ID RADAR INTERFEROMETRY; FIELD; STRAIN; WATER
AB One important issue in the storage of large volumes of fluids, mainly water and CO2, in the deep subsurface is to determine the resulting field-scale-induced displacements and consequences of overpressures on the mechanical integrity of the storage reservoir and surroundings. A quantifiable estimation of displacement can be made by combining the robust, cost-effective, and repeatable geophysical techniques of micro-gravimetry, differential global positioning system (DGPS), and differential synthetic aperture radar interferometry (DInSAR). These techniques were field tested and evaluated for the first time on an active large-volume aquifer storage and recovery (ASR) project in Pendleton, Oregon, USA, where three ASR wells are injecting up to 1.9 million m(3) year(-1) into basalt aquifers to a depth of about 150 m. Injection and recovery of water at the wells are accompanied by significant gravity anomalies and vertical deformation of the ground surface localized to the immediate surroundings of the injection wells as evidenced by DGPS and gravity measurements collected in 2011. At a larger scale, and between 2011 and 2013, DInSAR monitoring of the Pendleton area shows sub-centimetric deformation in the western part of the city and close to the injection locations associated with ASR cycle. Deformations are found to be temporally out phased with the injection and recovery events due to complex groundwater flow. A numerical simulation of the effect of the water injection gives results in good agreement with the observations and confirms the validity of the approach, which could be deployed in similar geological contexts to look at the mechanical effects of water and gas injections.
C1 [Bonneville, Alain; Strickland, Christopher; Dermond, Jeffrey; Fang, Yilin; Sullivan, Charlotte] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Heggy, Essam; Normand, Jonathan] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Bonneville, A (reprint author), Pacific NW Natl Lab, MSIN K6-84,POB 999, Richland, WA 99352 USA.
EM alain.bonneville@pnnl.gov
OI Bonneville, Alain/0000-0003-1527-1578
FU U.S. Department of Energy (US DOE) [DE-FC26-04NT42262]
FX This work was carried out within the Zero Emissions Research Technology
Center (ZERT) funded by the U.S. Department of Energy (US DOE), under
Award No. DE-FC26-04NT42262.
NR 38
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U1 1
U2 19
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0920-4741
EI 1573-1650
J9 WATER RESOUR MANAG
JI Water Resour. Manag.
PD OCT
PY 2015
VL 29
IS 13
BP 4667
EP 4682
DI 10.1007/s11269-015-1083-y
PG 16
WC Engineering, Civil; Water Resources
SC Engineering; Water Resources
GA CQ7UT
UT WOS:000360811200006
ER
PT J
AU Sainio, S
Palomaki, T
Tujunen, N
Protopopova, V
Koehne, J
Kordas, K
Koskinen, J
Meyyappan, M
Laurila, T
AF Sainio, Sami
Palomaki, Tommi
Tujunen, Noora
Protopopova, Vera
Koehne, Jessica
Kordas, Krisztian
Koskinen, Jari
Meyyappan, M.
Laurila, Tomi
TI Integrated Carbon Nanostructures for Detection of Neurotransmitters
SO MOLECULAR NEUROBIOLOGY
LA English
DT Article
DE Multiwalled carbon nanotubes; Carbon nanofibers; Dopamine;
Electrochemistry; Diamond-like carbon
ID RAT HIPPOCAMPAL SLICE; ELECTRODES; FILMS; STIMULATION; NANOTUBES;
BURDEN; GROWTH; ARRAYS; BRAIN; LAYER
AB Carbon-based materials, such as diamond-like carbon (DLC), carbon nanofibers (CNFs), and carbon nanotubes (CNTs), are inherently interesting for neurotransmitter detection due to their good biocompatibility, low cost and relatively simple synthesis. In this paper, we report on new carbon-hybrid materials, where either CNTs or CNFs are directly grown on top of tetrahedral amorphous carbon (ta-C). We show that these hybrid materials have electrochemical properties that not only combine the best characteristics of the individual "building blocks" but their synergy makes the electrode performance superior compared to conventional carbon based electrodes. By combining ta-C with CNTs, we were able to realize electrode materials that show wide and stable water window, almost reversible electron transfer properties and high sensitivity and selectivity for detecting dopamine in the presence of ascorbic acid. Furthermore, the sensitivity of ta-C + CNF hybrids towards dopamine as well as glutamate has been found excellent paving the road for actual in vivo measurements. The wide and stable water window of these sensors enables detection of other neurotransmitters besides DA as well as capability of withstanding higher potentials without suffering from oxygen and hydrogen evolution.
C1 [Sainio, Sami; Palomaki, Tommi; Tujunen, Noora; Laurila, Tomi] Aalto Univ, Sch Elect Engn, Dept Elect Engn & Automat, Espoo 02150, Finland.
[Protopopova, Vera; Koskinen, Jari] Aalto Univ, Sch Chem Technol, Dept Mat Sci, Espoo 02150, Finland.
[Sainio, Sami; Koehne, Jessica; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Kordas, Krisztian] Univ Oulu, Dept Elect Engn, FIN-90570 Oulu, Finland.
RP Sainio, S (reprint author), Aalto Univ, Sch Elect Engn, Dept Elect Engn & Automat, Espoo 02150, Finland.
EM sami.sainio@aalto.fi
RI Koskinen, Jari/J-3886-2014; Kordas, Krisztian/E-7654-2015; Laurila,
Tomi/B-2076-2013;
OI Palomaki, Tommi/0000-0002-6605-8593
NR 19
TC 5
Z9 5
U1 4
U2 31
PU HUMANA PRESS INC
PI TOTOWA
PA 999 RIVERVIEW DRIVE SUITE 208, TOTOWA, NJ 07512 USA
SN 0893-7648
EI 1559-1182
J9 MOL NEUROBIOL
JI Mol. Neurobiol.
PD OCT
PY 2015
VL 52
IS 2
SI SI
BP 859
EP 866
DI 10.1007/s12035-015-9233-z
PG 8
WC Neurosciences
SC Neurosciences & Neurology
GA CQ6AQ
UT WOS:000360687200006
PM 26093378
ER
PT J
AU Ceresa, M
Mangado, N
Andrews, RJ
Ballester, MA
AF Ceresa, Mario
Mangado, Nerea
Andrews, Russell J.
Gonzalez Ballester, Miguel A.
TI Computational Models for Predicting Outcomes of Neuroprosthesis
Implantation: the Case of Cochlear Implants
SO MOLECULAR NEUROBIOLOGY
LA English
DT Article
DE Computational models; Finite element analysis; Cochlear implants; Deep
brain stimulation
ID DEEP BRAIN-STIMULATION; FUTURE
AB Electrical stimulation of the brain has resulted in the most successful neuroprosthetic techniques to date: deep brain stimulation (DBS) and cochlear implants (CI). In both cases, there is a lack of pre-operative measures to predict the outcomes after implantation. We argue that highly detailed computational models that are specifically tailored for a patient can provide useful information to improve the precision of the nervous system electrode interface. We apply our framework to the case of CI, showing how we can predict nerve response for patients with both intact and degenerated nerve fibers. Then, using the predicted response, we calculate a metric for the usefulness of the stimulation protocol and use this information to rerun the simulations with better parameters.
C1 [Ceresa, Mario; Mangado, Nerea; Gonzalez Ballester, Miguel A.] Univ Pompeu Fabra, Simbiosys Grp, Barcelona, Spain.
[Andrews, Russell J.] NASA, Ames Res Ctr, Smart Syst & Nanotechnol, Moffett Field, CA 94035 USA.
[Gonzalez Ballester, Miguel A.] ICREA, Barcelona, Spain.
RP Ceresa, M (reprint author), Univ Pompeu Fabra, Simbiosys Grp, Barcelona, Spain.
EM mario.ceresa@upf.edu
RI Gonzalez Ballester, Miguel Angel/D-1349-2013;
OI Gonzalez Ballester, Miguel Angel/0000-0002-9227-6826; Ceresa,
Mario/0000-0002-2410-0212
FU European Union Seventh Frame Programme [304857]
FX The research leading to these results received funding from the European
Union Seventh Frame Programme (FP7/2007-2013) under grant agreement
304857.
NR 19
TC 4
Z9 4
U1 1
U2 6
PU HUMANA PRESS INC
PI TOTOWA
PA 999 RIVERVIEW DRIVE SUITE 208, TOTOWA, NJ 07512 USA
SN 0893-7648
EI 1559-1182
J9 MOL NEUROBIOL
JI Mol. Neurobiol.
PD OCT
PY 2015
VL 52
IS 2
SI SI
BP 934
EP 941
DI 10.1007/s12035-015-9257-4
PG 8
WC Neurosciences
SC Neurosciences & Neurology
GA CQ6AQ
UT WOS:000360687200012
PM 26084438
ER
PT J
AU Madansingh, S
Bloomberg, JJ
AF Madansingh, S.
Bloomberg, J. J.
TI Understanding the effects of spaceflight on head-trunk coordination
during walking and obstacle avoidance
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Head-trunk coordination; En bloc; Latency; Unloading; Bed rest;
Vestibular-somatosensory convergence
ID LONG-DURATION SPACEFLIGHT; SPACE-FLIGHT; ORTHOSTATIC INTOLERANCE;
PARKINSONS-DISEASE; BED REST; TURNS; STRATEGIES; LOCOMOTION;
MICROGRAVITY; COUNTERMEASURE
AB Prolonged exposure to spaceflight conditions results in a battery of physiological changes, some of which contribute to sensorimotor and neurovestibular deficits. Upon return to Earth, functional performance changes are tested using the Functional Task Test (FIT), which includes an obstacle course to observe post-flight balance and postural stability, specifically during turning. The goal of this study was to quantify changes in movement strategies during turning events by observing the latency between head-and-trunk coordinated movements. It was hypothesized that subjects experiencing neurovestibular adaptations would exhibit head-to-trunk locking ('en bloc' movement) during turning, exhibited by a decrease in latency between head and trunk movement. FIT data samples were collected from 13 ISS astronauts and 26 male 70-day head down tilt bed rest subjects, including bed rest controls (10 BRC) and bed rest exercisers (16 BRE). Samples were analyzed three times pre-exposure, immediately post-exposure (0 or 1-day post) and 2-3 times during recovery from the unloading environment Two 3D inertial measurements units (XSens MTx) were attached to subjects, one on the head and one on the upper back. This study focused primarily on the yaw movements about the subject's center of rotation. Time differences (latency) between head and trunk movement were averaged across a slalom obstacle portion, consisting of three turns (approximately three 60 turns). All participants were grouped as 'decreaser' or 'increaser', relating to their change in head-to-trunk movement latency between pre- and post-environmental adaptation measures. Spaceflight unloading (ISS) showed a bimodal response between the 'increaser' and 'decreaser' group, while both bed rest control (BRC) and bed rest exercise (BRE) populations showed increased preference towards a 'decreaser' categorization, displaying greater head-trunk locking. It is clear that changes in movement strategies are adopted during exposure to an unloading environment. These results further the understanding of vestibular-somatosensory convergence and support the use of bed rest as an exclusionary model to better understand sensorimotor changes in spaceflight. (C) 2015 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Madansingh, S.] Univ Houston, Dept Hlth & Human Performance, Houston, TX 77004 USA.
[Bloomberg, J. J.] NASA, Lyndon B Johnson Space Ctr, Neurosci Lab, Houston, TX 77058 USA.
RP Madansingh, S (reprint author), Univ Houston, Dept Hlth & Human Performance, Houston, TX 77004 USA.
EM simadansingh@uh.edu; jacob.j.bloomberg@nasa.gov
NR 39
TC 1
Z9 1
U1 4
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT-NOV
PY 2015
VL 115
BP 165
EP 172
DI 10.1016/j.actaastro.2015.05.022
PG 8
WC Engineering, Aerospace
SC Engineering
GA CP4TU
UT WOS:000359876300016
ER
PT J
AU Johannsson, M
Wen, A
Kraetzig, B
Cohen, D
Liu, DP
Liu, H
Palencia, H
Wagner, H
Stotesbury, I
Jaworski, J
Tallineau, J
Laib, K
Dubois, LE
Lander, M
Claude, M
Shouppe, M
Gallagher, M
Brogan, M
Brito, NL
Cyr, P
Ewing, R
Marcu, SD
Bareksten, S
Suma, MN
Sreerekha, U
Sharma, T
Li, TT
Yang, W
Chen, WS
Ricard, W
van Meerbeeck, W
Cui, Y
Trolley, Z
Zhao, ZG
AF Johannsson, Magni
Wen, Anne
Kraetzig, Benjamin
Cohen, Dan
Liu, Dapeng
Liu, Hao
Palencia, Hilda
Wagner, Hugo
Stotesbury, Ian
Jaworski, Jaroslaw
Tallineau, Julien
Laib, Karima
Dubois, Louis-Etienne
Lander, Mark
Claude, Matthew
Shouppe, Matthew
Gallagher, Michael
Brogan, Mitchell
Brito, Natalia Larrea
Cyr, Philippe
Ewing, Rory
Marcu, Sebastian Davis
Bareksten, Silje
Suma, M. N.
Sreerekha, U.
Sharma, Tanay
Li, Tiantian
Yang, Wei
Chen, Wensheng
Ricard, William
van Meerbeeck, William
Cui, Yang
Trolley, Zac
Zhao, Zhigang
TI Space and Open Innovation: Potential, limitations and conditions of
success
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Open innovation; Space; Case study; Survey; Asteroid mining
ID COMPETITIVE ADVANTAGE; FIRM
AB The classical model of innovation behind closed doors is slowly but surely being challenged by the Open Innovation model that is reshaping the way organizations bring new products and services into the market. This paper reports on the results of an International Space University (ISU) Team Project (TP) focused on the potential, limitations and conditions of success of Open Innovation in the space sector using ISU's international, interdisciplinary, intercultural (3Is) approach. Open Innovation can be defined as "the process of strategically managing the sharing of ideas and resources among entities to co-create value". Conventional approaches to technology development for space, such as spin-offs or spin-ins, are no longer sufficient to fully describe the interactions between organizations in today's Research and Development (R&D) landscape. Traditionally, conducting space technology development and launching space missions required massive infrastructure investments, long lead times and large teams of experts. However, internal R&D, dedicated marketing departments and closely guarded intellectual property are no longer the only way to achieve success. Smaller, nimbler teams, significant use of crowdfunding, a more aggressive approach to managing risk and a great motivation to leverage intellectual property are just some of their defining characteristics. By using a case study methodology focused on asteroid mining supported by a critical literature review, the project team highlighted the potential of Open Innovation in space by identifying its most promising applications as well as its limitations. (C) 2015 Published by Elsevier Ltd. on behalf of IAA.
C1 [Johannsson, Magni] German Aerosp Ctr, Inst Space Syst, Space Launcher Syst Anal, D-28359 Bremen, Germany.
[Wen, Anne; Kraetzig, Benjamin; Liu, Dapeng; Liu, Hao; Wagner, Hugo; Stotesbury, Ian; Jaworski, Jaroslaw; Laib, Karima; Lander, Mark; Claude, Matthew; Shouppe, Matthew; Brogan, Mitchell; Brito, Natalia Larrea; Cyr, Philippe; Ewing, Rory; Suma, M. N.; Sreerekha, U.; Sharma, Tanay; Li, Tiantian; Yang, Wei; Chen, Wensheng; van Meerbeeck, William; Cui, Yang; Trolley, Zac; Zhao, Zhigang] Int Space Univ, F-67400 Strasbourg, France.
[Cohen, Dan] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Palencia, Hilda] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Tallineau, Julien] QinetiQ Space Nv, B-9150 Kruibeke, Belgium.
[Dubois, Louis-Etienne; Ricard, William] CGS MINES ParisTech, Mosaic HEC Montreal, Montreal, PQ H3T 2A7, Canada.
[Gallagher, Michael] Alberta Hlth Serv, Edmonton, AB T5J 3E4, Canada.
[Marcu, Sebastian Davis] Design & Data GmbH, D-50672 Cologne, Germany.
[Bareksten, Silje] Inven2 AS, N-0349 Oslo, Norway.
RP Johannsson, M (reprint author), German Aerosp Ctr, Inst Space Syst, Space Launcher Syst Anal, D-28359 Bremen, Germany.
EM magni.johannsson@dlr.de
FU NASA headquarters
FX The authors of the paper, its accompanying report and executive summary
are grateful to the following experts whose input and insights were
instrumental to the development of these documents: Adam Mizera,
Christian Sallaberger, Claire Jolly, David Grandadam, Denis Remon, Eric
Hall, Gary Martin, Gregg Maryniak, Ian Fichtenbaum, Jacques Arnould, Jim
Burke, Julio Aprea, Ken Davidian, Luise Weber-Steinhaus, Mario
Ciaramicoli, Maryam Nabavi, Matt Killick, Michael Labib, Patrick
Cohendet, Rene Oosterlinck and Simon "Pete" Worden. We would also like
to thank NASA headquarters for their generous sponsorship, as well as
Carol Carnett, Merryl Azriel, Nikita Marwaha and Bill S. Hamm for their
assistance. Lastly we would like to give special thanks to the project
chair Ozgur Gurtuna, without whose guidance and support it would have
been impossible to complete the project.
NR 40
TC 0
Z9 1
U1 7
U2 84
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT-NOV
PY 2015
VL 115
BP 173
EP 184
DI 10.1016/j.actaastro.2015.05.023
PG 12
WC Engineering, Aerospace
SC Engineering
GA CP4TU
UT WOS:000359876300017
ER
PT J
AU Babuscia, A
Cheung, KM
Divsalar, D
Lee, C
AF Babuscia, Alessandra
Cheung, Kar-Ming
Divsalar, Dariush
Lee, Charles
TI Development of cooperative communication techniques for a network of
small satellites and CubeSats in deep space: The SOLARA/SARA test case
SO ACTA ASTRONAUTICA
LA English
DT Article
DE CubeSat; Communication; Interplanetary; Array; CDMA; Beam-forming
ID DESIGN
AB In the last decade, great progress was made in the development of small satellites and CubeSats. Several small spacecraft were designed, fabricated, launched, and successfully operated in low Earth orbit. While more companies and space agencies are becoming interested in CubeSats and small satellite, also the mission goals for these spacecraft are gradually changing: these small spacecraft are starting to be considered for deep-space, interplanetary exploration.
Given the limited size, mass and power capabilities of these small platforms, one of the most interesting problems to address is how to develop a communication system to allow small satellites to communicate from very far distance in the solar system.
This paper aims to address this problem by proposing cooperative communication approaches in which multiple CubeSats communicate cooperatively together to improve the link performance with respect to the case of a single satellite transmitting. Three approaches are proposed: a beam-forming approach, a coding approach, and a network approach. The approaches are applied to the specific case of the SOLARA/SARA concept: a proposed constellation of CubeSats at the Lunar Lagrangian point L1 which aims to perform radio astronomy at very low frequencies (30 kHz to 3 MHz). The paper describes the development of the approaches, the simulation and a graphical user interface developed in Matlab which allows to perform trade-offs across multiple constellation's configurations. (C) 2015 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Babuscia, Alessandra; Cheung, Kar-Ming; Divsalar, Dariush; Lee, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Babuscia, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Alessandra.Babuscia@jpl.nasa.gov; Kar-Ming.Cheung@jpl.nasa.gov;
Dariush.Divsalar@jpl.nasa.gov; Charles.Lee@jpl.nasa.gov
NR 20
TC 0
Z9 0
U1 4
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT-NOV
PY 2015
VL 115
BP 349
EP 355
DI 10.1016/j.actaastro.2015.06.001
PG 7
WC Engineering, Aerospace
SC Engineering
GA CP4TU
UT WOS:000359876300034
ER
PT J
AU Schonberg, WP
Ratliff, JM
AF Schonberg, William P.
Ratliff, J. Martin
TI Hypervelocity impact of a pressurized vessel: Comparison of ballistic
limit equation predictions with test data and rupture limit equation
development
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Pressurized vessel; Propellant tank; Orbital debris; MMOD; Ballistic
limit equation; Catastrophic failure
AB Most spacecraft have at least one pressurized vessel on board. For robotic spacecraft, it is usually a liquid propellant tank. One of the design considerations of such spacecraft is the possible damage that might occur in the event of an on-orbit impact by a micro-meteoroid or orbital debris (MMOD) particle. While considerable effort has been expended in the study of the response of non-pressurized spacecraft components to these kinds of impacts, relatively few studies have been conducted on the pressurized elements of such spacecraft. This paper presents the results of a study performed to address the following aspects of this problem: how well current ballistic limit equations predict impact-induced perforation damage that might occur in pressurized spacecraft components such as tanks; and, the development of data-driven rupture limit equations that can be used to differentiate between impact conditions that would result in only a small hole or crack, from those that would cause catastrophic tank failure. This information would be useful to a design engineer who might be able to select tank materials to avoid catastrophic tank failure in the event of a perforating on-orbit MMOD particle impact. Tank perforation would typically result in a failed mission; and catastrophic tank failure might generate multiple pieces of new debris, increasing the risk to other spacecraft. (C) 2015 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Schonberg, William P.] Missouri Univ Sci & Technol, Rolla, MO 65409 USA.
[Ratliff, J. Martin] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Schonberg, WP (reprint author), Missouri Univ Sci & Technol, Rolla, MO 65409 USA.
EM wschon@mst.edu
FU NASA/Jet Propulsion Laboratory
FX The authors wish to extend their gratitude to the NASA/Jet Propulsion
Laboratory for providing the support that made this study possible.
NR 23
TC 0
Z9 0
U1 1
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT-NOV
PY 2015
VL 115
BP 400
EP 406
DI 10.1016/j.actaastro.2015.06.013
PG 7
WC Engineering, Aerospace
SC Engineering
GA CP4TU
UT WOS:000359876300040
ER
PT J
AU Blakey, T
Melesse, AM
Rousseaux, CS
AF Blakey, Tara
Melesse, Assefa M.
Rousseaux, Cecile S.
TI Toward connecting subtropical algal blooms to freshwater nutrient
sources using a long-term, spatially distributed, in situ chlorophyll-a
record
SO CATENA
LA English
DT Article
DE Tropical environment; Eutrophication; Chl-a; Florida Bay; Nutrients;
Algal blooms
ID INNER-SHELF LAGOON; FLORIDA-BAY; SOUTHWEST FLORIDA; COASTAL WATERS; USA;
QUALITY; EUTROPHICATION; CYANOBACTERIA; VARIABILITY; EVERGLADES
AB Harmful algal blooms are increasing in tropical estuaries which can have complex morphologies and hydrologic regimes while being less well studied than temperate estuaries. Spatial and temporal patterns of algal bloom occurrence in Florida Bay were examined to evaluate the potential contribution of the various freshwater inputs to the subtropical bay as nutrient sources. Monthly water quality data, from 1989 to 2009, at 28 sampling stations across the bay were analyzed at the station-month level, aggregated into hydrologic Zones of Similar Influence and based on annual rainfall seasons. The Zones of Similar Influence are linked to the geomorphology of the bay with western areas being more directly connected to the Southwest Florida Shelf waters than eastern areas. Correlation analysis suggested that inputs of phosphorus were the predominant factor in the initiation of elevated chlorophyll a (chl-a) levels but was also consistent with higher nitrogen limitation in western Florida Bay as reported in literature. Differences in mean monthly chl-a indicated a seasonality of algal blooms with elevated chl-a concentrations following heavy precipitation months for stations in the north-central and western areas of the bay where algal blooms have been re-occurring. Differences in stations' chl-a concentrations showed stations to the northwest as having significantly higher concentrations than more interior stations during the dry season but not during the rainy season (when algal blooms are occurring). Mapping the sampling stations atop the bathymetry of Florida Bay highlighted the importance of coastal morphology in evaluation of potential nutrient pathways for estuarine algal bloom sources. The specific factors resulting in the seasonal cycles of blooms remained unresolved but portions of the bay and times of year were identified as important areas for further research. This study indicates that illustrating the interplay of geomorphology and winds and rains at fine temporal and spatial resolution is required to describe nutrient circulation for systems with complex morphologies such as those associated with reefs, island matrices and headlands. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Blakey, Tara; Melesse, Assefa M.] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA.
[Rousseaux, Cecile S.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Rousseaux, Cecile S.] Univ Space Res Assoc, Columbia, MD USA.
RP Melesse, AM (reprint author), Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA.
EM tblakey@fiu.edu; melessea@fiu.edu; Cecile.S.Rousseaux@nasa.gov
RI Melesse, Assefa/F-9931-2013; Rousseaux, Cecile/E-8811-2012
OI Melesse, Assefa/0000-0003-4724-9367; Rousseaux,
Cecile/0000-0002-3022-2988
FU National Aeronautics and Space Administration (NASA) Minority University
Research and Education, WaterSCAPES, Program [NNX-10AQ13A]
FX This research was conducted through the support of the National
Aeronautics and Space Administration (NASA) Minority University Research
and Education, WaterSCAPES, Program (Grant No. NNX-10AQ13A). Special
thanks to Florida International University's Graduate School Statistical
Consulting Services, and the Southeast Environmental Research Center
(SERC) for their contributions to this work.
NR 39
TC 0
Z9 0
U1 1
U2 47
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0341-8162
EI 1872-6887
J9 CATENA
JI Catena
PD OCT
PY 2015
VL 133
BP 119
EP 127
DI 10.1016/j.catena.2015.05.001
PG 9
WC Geosciences, Multidisciplinary; Soil Science; Water Resources
SC Geology; Agriculture; Water Resources
GA CP5YD
UT WOS:000359960600012
ER
PT J
AU Hurwitz, D
Kring, DA
AF Hurwitz, Debra
Kring, David A.
TI Potential sample sites for South Pole-Aitken basin impact melt within
the Schrodinger basin
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE South Pole-Aitken basin; Schrodinger basin; lunar cataclysm; lunar
exploration; lunar landing sites
ID LUNAR-SURFACE; MOON; EXPLORATION; MISSION; BOMBARDMENT; PROSPECTOR;
CATACLYSM; VOLUMES; GEOLOGY; MANTLE
AB Determining the age of the South Pole-Aitken (SPA) basin ranks among the highest priorities in lunar science. This datum would constrain the timing of the oldest and largest basin-forming event on the Moon, information that is essential to any evaluation of the collisional evolution of the early Solar System. To locate material that preserves the age of SPA, a geochemical model of SPA impact melt is integrated with chemical and mineralogical analyses of the lunar surface determined from orbit. Results suggest the southern wall of Schrodinger basin contains material with the mineralogical and geochemical signatures of SPA melt and, thus, represents a candidate destination for sampling material that can constrain the age of the SPA impact. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Hurwitz, Debra; Kring, David A.] Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, Houston, TX 77058 USA.
[Hurwitz, Debra; Kring, David A.] Lunar & Planetary Inst, Solar Syst Explorat Res Virtual Inst, Houston, TX 77058 USA.
RP Hurwitz, D (reprint author), Oak Ridge Associated Univ, NASA Goddard Space Flight Ctr, Planetary Geodynam Lab Code 698, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM debra.m.hurwitz@nasa.gov; kring@lpi.usra.edu
FU Solar System Exploration Research Virtual Institute [NNA14AB07A]
FX This work was supported by Solar System Exploration Research Virtual
Institute contract NNA14AB07A (PI David A. Kring). LPI Contribution No.
1854.
NR 46
TC 3
Z9 3
U1 0
U2 3
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 OCT 1
PY 2015
VL 427
BP 31
EP 36
DI 10.1016/j.epsl.2015.06.055
PG 6
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CO7HS
UT WOS:000359330800004
ER
PT J
AU Chen, Y
Zhang, YX
Liu, Y
Guan, YB
Eiler, J
Stolper, EM
AF Chen, Yang
Zhang, Youxue
Liu, Yang
Guan, Yunbin
Eiler, John
Stolper, Edward M.
TI Water, fluorine, and sulfur concentrations in the lunar mantle
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE moon; melt inclusions; volatiles; water; H2O/Ce ratio; F/Nd ratio
ID HOSTED MELT INCLUSIONS; OCEAN-RIDGE BASALT; VOLATILE ABUNDANCES;
TERRESTRIAL PLANETS; OXYGEN FUGACITY; MOONS INTERIOR; TRACE-ELEMENTS;
ORIGIN; MAGMA; H2O
AB The concentrations of volatile elements in the moon have important implications for the formation of the earth-moon system. There is currently a debate regarding the water content of the lunar mantle: Authors studying H2O in lunar pyroclastic glass beads and in olivine-hosted melt inclusions in such pyroclastic samples and in plagioclase crystals in lunar highland anorthosites infer hundreds of ppm H2O in the lunar mantle. In contrast, authors studying Zn/Fe ratios infer that the H2O concentration in the lunar mantle is <= 1 ppm, and they argue that the glassy lunar basalts are a local anomaly. We contribute to a resolution of the debate by a broader examination of the concentrations of H2O and other volatile components in olivine-hosted melt inclusions in a wider range of lunar mare basalts, including crystalline melt inclusions that are homogenized by melting in the laboratory. We find that F, Cl, and S concentrations in various lunar melt inclusions (including those in glassy lunar basalts) are similar to one another, and previously studied glassy lunar basalts are not a local anomaly in terms of these volatile concentrations. Furthermore, we estimate the pre-degassing H2O/Ce, F/Nd, and S/Dy ratios of mare basaltic magmas to be at least 64, 4.0 and 100 respectively. These ratios are lower than those of primitive earth mantle by a factor of 3, 5, and 4 respectively. The depletion factors of these volatile elements relative to the earth's primitive mantle do not correlate strongly with volatility or bonding energy, and indeed they are roughly constant and similar to those of other volatile elements such as Li, Cs, Rb and K. This approximate constancy of volatile depletion in the moon relative to the earth can be explained by assuming that both the earth and the moon acquired volatiles from a similar source or by a similar mechanism but the earth was more efficient in acquiring the volatiles. We estimate the H2O, F and S concentrations in the primitive lunar mantle source to be at least 110, 5.3, and 70 Pim. respectively - similar to or slightly lower than those in terrestrial MORB mantle. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Chen, Yang; Zhang, Youxue] Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA.
[Chen, Yang; Liu, Yang] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Guan, Yunbin; Eiler, John; Stolper, Edward M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Chen, Y (reprint author), Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA.
EM Yang.Chen@jpl.nasa.gov; youxue@umich.edu
OI Zhang, Youxue/0000-0002-7439-0086; Chen, Yang/0000-0003-4729-3499
FU NASA [NNX10AH74G, NNX15AH37G, NNN13D465T, NNX12AH63G]; University of
Michigan; Jet Propulsion Laboratory
FX We thank NASA CAPTEM for providing the lunar samples, K.P. Jochum for
providing the MPI-Ding glass standards, F. Albarede, Cin-Ty Lee, and
three anonymous reviewers for comments. This research is supported by
NASA grants NNX10AH74G and NNX15AH37G, and University of Michigan funds.
YL acknowledges NASA grant NNN13D465T and support from Jet Propulsion
Laboratory, which is managed by California Institute of Technology under
a contract with NASA. EMS acknowledges NASA grant NNX12AH63G.
NR 72
TC 13
Z9 13
U1 8
U2 35
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 OCT 1
PY 2015
VL 427
BP 37
EP 46
DI 10.1016/j.epsl.2015.06.046
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CO7HS
UT WOS:000359330800005
ER
PT J
AU Zahnle, KJ
Lupu, R
Dobrovolskis, A
Sleep, NH
AF Zahnle, Kevin J.
Lupu, Roxana
Dobrovolskis, Anthony
Sleep, Norman H.
TI The tethered Moon
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Earth atmospheric evolution; Earth thermal evolution; Earth and Moon
formation; Earth and Moon tidal evolution
ID STRONG TIDAL DISSIPATION; GIANT IMPACT; MAGMA OCEAN; ORBITAL
INCLINATION; LUNAR ACCRETION; SOLAR-SYSTEM; EARTH; EVOLUTION; ORIGIN;
ATMOSPHERES
AB We address the thermal history of the Earth after the Moon-forming impact, taking tidal heating and thermal blanketing by the atmosphere into account. The atmosphere sets an upper bound of similar to 100 W/m(2) on how quickly the Earth can cool. The liquid magma ocean cools over 2-10 Myr, with longer times corresponding to high angular-momentum events. Tidal heating is focused mostly in mantle materials that are just beginning to freeze. The atmosphere's control over cooling sets up a negative feedback between viscosity-dependent tidal heating and temperature-dependent viscosity of the magma ocean. While the feedback holds, evolution of the Moon's orbit is limited by the modest radiative cooling rate of Earth's atmosphere. Orbital evolution is orders of magnitude slower than in conventional constant Q models, which promotes capture by resonances. The evection resonance is encountered early, when the Earth is molten. Capture by the evection resonance appears certain but unlikely to generate much eccentricity because it is encountered early when the Earth is molten and Q(circle plus) >> Q((sic)). Tidal dissipation in the Earth becomes more efficient Q(circle plus) >> Q((sic)) later when the Moon is between 20120 and similar to 40R(circle plus). If lunar eccentricity grew great, this was when it did so, perhaps setting the table for some other process to leave its mark on the inclination of the Moon. Published by Elsevier B.V.
C1 [Zahnle, Kevin J.] NASA Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Lupu, Roxana; Dobrovolskis, Anthony] SETI Inst, Mountain View, CA 95064 USA.
[Sleep, Norman H.] Stanford Univ, Dept Geophys, Stanford, CA 94305 USA.
RP Zahnle, KJ (reprint author), NASA Ames Res Ctr, Div Space Sci, MS 245-3, Moffett Field, CA 94035 USA.
EM Kevin.J.Zahnle@NASA.gov; roxana.s.lupu@nasa.gov;
anthony.r.dobrovolskis@nasa.gov; norm@stanford.edu
FU NASA Planetary Atmospheres Program
FX The authors thank Michael Efroimsky and an anonymous referee for helpful
comments. We thank the NASA Planetary Atmospheres Program for support of
this work.
NR 50
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U1 2
U2 27
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 OCT 1
PY 2015
VL 427
BP 74
EP 82
DI 10.1016/j.epsl.2015.06.058
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CO7HS
UT WOS:000359330800009
ER
PT J
AU Byrne, PK
Klimczak, C
McGovern, PJ
Mazarico, E
James, PB
Neumann, GA
Zuber, MT
Solomon, SC
AF Byrne, Paul K.
Klimczak, Christian
McGovern, Patrick J.
Mazarico, Erwan
James, Peter B.
Neumann, Gregory A.
Zuber, Maria T.
Solomon, Sean C.
TI Deep-seated thrust faults bound the Mare Crisium lunar mascon
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE GRAIL; LRO; Mare Crisium; mascon; Moon; thrust faults
ID GRAVITY-FIELD; BASINS; MOON; ORIGIN; GRAIL; SLIP; TECTONICS; EVOLUTION;
MISSION; MERCURY
AB Mare Crisium is composed of a set of volcanic deposits situated in an impact basin on the Moon's near side. The topography of the mare is dominated by an annulus of elevated topography, the inner edge of which is delineated by basin-concentric wrinkle ridges. From a combination of remotely sensed image and topographic data and numerical modeling, we show that the thrust faults that underlie these ridges penetrate up to 20 km in depth, considerably below the base of the mare deposits themselves. Thrust faults of this scale have not heretofore been recognized on the Moon. Mare Crisium sits above a region of uplifted mantle, which contributes to a mass excess beneath the basin, and we demonstrate by comparison with free-air gravity anomaly and derived crustal thickness data for Crisium that the thrust faults structurally bound this elevated mantle material. By means of finite-element models of stresses induced by lithospheric loading within the basin, we argue that the deep-seated thrusts may have been localized by the boundary between the superisostatic mantle material and a sub-isostatic collar of thickened crust that resulted from basin formation and modification shortly after impact. Importantly, numerous other mare-filled mascon basins on the Moon share the same topographic and tectonic characteristics as Crisium, suggesting that they, too, are underlain by deep-seated thrust faults that formed in a similar manner. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Byrne, Paul K.; McGovern, Patrick J.] Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX 77058 USA.
[Byrne, Paul K.; Klimczak, Christian; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Klimczak, Christian] Univ Georgia, Dept Geol, Athens, GA 30602 USA.
[Mazarico, Erwan; Neumann, Gregory A.] NASA Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[James, Peter B.; Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Byrne, PK (reprint author), Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX 77058 USA.
EM byrne@lpi.usra.edu
RI Neumann, Gregory/I-5591-2013; Mazarico, Erwan/N-6034-2014;
OI Neumann, Gregory/0000-0003-0644-9944; Mazarico,
Erwan/0000-0003-3456-427X; McGovern, Patrick/0000-0001-9647-3096
FU NASA GRAIL [NNM08AA18C]; NASA MESSENGER [NASW-00002]; NASA LASER Program
[NNX13AJ60G]
FX We are grateful for comments on earlier versions of this paper from two
anonymous reviewers. We acknowledge support from the NASA GRAIL project,
under contract NNM08AA18C to the Massachusetts Institute of Technology,
and from the NASA MESSENGER project, under contract NASW-00002 to the
Carnegie Institution of Washington. PJM received support from a NASA
LASER Program grant (NNX13AJ60G). We thank Patrick J. Gillen for
assistance with the goodness-of-fit analysis of the model fault
displacement profiles. This research made use of NASA's Planetary Data
System and Astrophysics Data System.
NR 39
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U1 0
U2 10
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 OCT 1
PY 2015
VL 427
BP 183
EP 190
DI 10.1016/j.epsl.2015.06.022
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CO7HS
UT WOS:000359330800019
ER
PT J
AU Campbell, MD
Pollack, AG
Gledhill, CT
Switzer, TS
DeVries, DA
AF Campbell, Matthew D.
Pollack, Adam G.
Gledhill, Christopher T.
Switzer, Theodore S.
DeVries, Douglas A.
TI Comparison of relative abundance indices calculated from two methods of
generating video count data
SO FISHERIES RESEARCH
LA English
DT Article
DE Video; BRUV; MaxN; MeanCount; Relative abundance index; Catchability
ID GULF-OF-MEXICO; REEF FISH; GEOGRAPHIC-DISTRIBUTION; SOUTHERN GULF;
ST-LAWRENCE; UNIT-EFFORT; SYSTEM; FISHERIES; DENSITY; MODELS
AB The use of baited remote underwater video to remotely observe fish and generate indices of relative abundance has steadily gained acceptance as a fisheries management tool particularly as survey time series have matured. Because 'capture' for this gear is visually derived, fish can possibly be counted multiple times and therefore different methods of estimating site abundances have been developed. We compared the performance of two video abundance estimation techniques, MaxN and MeanCount, by generating relative indices of abundance using a delta lognormal model. We demonstrated high correspondence between standardized indices produced through the years analyzed independent of the species evaluated, indicating there was little change in the information content between indices. Despite the agreement between the indices, estimates for proportion positive and coefficient of variation (CV) showed a general reduction in precision when using the MeanCount method for all species analyzed. Systematic underestimation of proportion positives and high CV values generated using MeanCount is problematic for the use of that abundance estimation method. Individual-based modeling results confirmed that MeanCount is linearly related to true abundance, while MaxN showed a power relationship. However, the MaxN estimate became linear as the area observed was increased in the model from 25% to 100%, which suggests that syncing cameras and generating counts over the entire observed area would eliminate the asymptotic relationship and simplify the use of MaxN estimators. Better understanding of catchability for optical type gears would enhance understanding of the relationship between the generated index and true population abundance, and supply assessment scientist with a clearer understanding of how to incorporate these types of survey data into assessments. Published by Elsevier B.V.
C1 [Campbell, Matthew D.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA.
[Pollack, Adam G.] Riverside Technol Inc, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA.
[Gledhill, Christopher T.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Stennis Branch, Mississippi Labs, Stennis Space Ctr, MS 39529 USA.
[Switzer, Theodore S.] Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, St Petersburg, FL 33701 USA.
[DeVries, Douglas A.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Panama City Lab, Panama City, FL 32408 USA.
RP Campbell, MD (reprint author), Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, 3209 Frederic St, Pascagoula, MS 39567 USA.
EM matthew.d.campbell@noaa.gov
NR 38
TC 5
Z9 5
U1 9
U2 24
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0165-7836
EI 1872-6763
J9 FISH RES
JI Fish Res.
PD OCT
PY 2015
VL 170
BP 125
EP 133
DI 10.1016/j.fishres.2015.05.011
PG 9
WC Fisheries
SC Fisheries
GA CO3BZ
UT WOS:000359032900016
ER
PT J
AU Wang, S
Li, ZZ
Zhang, Y
Cheong, BL
Li, LH
AF Wang, Shang
Li, Zhengzheng
Zhang, Yan
Cheong, Boonleng
Li, Lihua
TI Implementation of Adaptive Pulse Compression in Solid-State Radars:
Practical Considerations
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Adaptive pulse compression (APC); multimission radar; solid-state radar
ID LEAST-SQUARES
AB This letter summarizes the applications of adaptive pulse compression (APC) in example solid-state radars for different missions. The radar examples include an X-band PX-1000 ground radar for severe weather observation, a Ku-band airborne radar for near-surface precipitation measurement, and an X-band radar experiment for air traffic observation. Representative APC algorithms are compared in terms of target estimation performance. In order to achieve the benefits of APC in actual radars, some important tradeoffs and considerations such as waveform template, sampling scheme, and noise estimation are discussed.
C1 [Wang, Shang; Li, Zhengzheng; Zhang, Yan; Cheong, Boonleng] Univ Oklahoma, Adv Radar Res Ctr, Intelligent Aerosp Radar Team, Norman, OK 73019 USA.
[Li, Lihua] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wang, S (reprint author), Univ Oklahoma, Adv Radar Res Ctr, Intelligent Aerosp Radar Team, Norman, OK 73019 USA.
EM lihua.li-1@nasa.gov
FU National Aeronautics and Space Administration [NNX11AM10A]
FX This work was supported by the National Aeronautics and Space
Administration under Grant NNX11AM10A.
NR 12
TC 0
Z9 0
U1 1
U2 4
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 OCT
PY 2015
VL 12
IS 10
BP 2170
EP 2174
DI 10.1109/LGRS.2015.2454481
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 CP0PD
UT WOS:000359576400033
ER
PT J
AU Bernardin, J
Chiaramonte, F
Dhir, V
Galloway, J
Goodson, K
Incropera, F
Kabov, O
Kaviany, M
Kazimi, M
Khusid, B
Kim, J
Kim, SM
Lee, J
Minkowycz, WJ
Qu, WL
Rose, J
Sammakia, B
Stephan, P
Vafai, K
Wen, CD
AF Bernardin, John
Chiaramonte, Francis
Dhir, Vijay
Galloway, Jesse
Goodson, Ken
Incropera, Frank
Kabov, Oleg
Kaviany, Massoud
Kazimi, Mujid
Khusid, Boris
Kim, Jungho
Kim, Sung-Min
Lee, Jaeseon
Minkowycz, W. J.
Qu, Weilin
Rose, John
Sammakia, Bahgat
Stephan, Peter
Vafai, Kambiz
Wen, Chang-Da
TI Professor Issam Mudawar on his 60th birthday
SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER
LA English
DT Biographical-Item
C1 [Bernardin, John] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Chiaramonte, Francis] NASA, Washington, DC USA.
[Dhir, Vijay] Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
[Galloway, Jesse] Amkor Technol, Tempe, AZ USA.
[Goodson, Ken] Stanford Univ, Stanford, CA 94305 USA.
[Incropera, Frank] Univ Notre Dame, Notre Dame, IN 46556 USA.
[Kabov, Oleg] Kutateladze Inst Thermophys, Novosibirsk, Russia.
[Kaviany, Massoud] Univ Michigan, Ann Arbor, MI 48109 USA.
[Kazimi, Mujid] MIT, Cambridge, MA 02139 USA.
[Khusid, Boris] New Jersey Inst Technol, Newark, NJ 07102 USA.
[Kim, Jungho] Univ Maryland, College Pk, MD USA.
[Kim, Sung-Min] Sungkyunkwan Univ, Seoul, South Korea.
[Lee, Jaeseon] Ulsan Natl Inst Sci & Technol, Ulsan, South Korea.
[Minkowycz, W. J.] Univ Illinois, Chicago, IL USA.
[Qu, Weilin] Univ Hawaii Manoa, Dept Mech Engn, Honolulu, HI 96822 USA.
[Rose, John] Univ London, London WC1E 7HU, England.
[Sammakia, Bahgat] Binghamton Univ, Binghamton, NY USA.
[Stephan, Peter] Tech Univ Darmstadt, Darmstadt, Germany.
[Vafai, Kambiz] Univ Calif Riverside, Riverside, CA 92521 USA.
[Wen, Chang-Da] Natl Cheng Kung Univ, Tainan 70101, Taiwan.
RP Qu, WL (reprint author), Univ Hawaii Manoa, Dept Mech Engn, Honolulu, HI 96822 USA.
EM qu@hawaii.edu
RI Kabov, Oleg /H-4519-2016
OI Kabov, Oleg /0000-0001-9720-4672
NR 1
TC 0
Z9 0
U1 3
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0017-9310
EI 1879-2189
J9 INT J HEAT MASS TRAN
JI Int. J. Heat Mass Transf.
PD OCT
PY 2015
VL 89
BP A1
EP A3
DI 10.1016/j.ijheatmasstransfer.2015.05.059
PG 3
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA CO3AV
UT WOS:000359029600001
ER
PT J
AU Brill, RW
Bushnell, PG
Elton, TA
Small, HJ
AF Brill, Richard W.
Bushnell, Peter G.
Elton, Timothy A.
Small, Hamish J.
TI The ability of blue crab (Callinectes sapidus, Rathbun 1886) to sustain
aerobic metabolism during hypoxia
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Digestion; Exercise; Hematodinium; Oxygen; SDA; Temperature
ID NEUSE RIVER ESTUARY; OXYGEN-CONSUMPTION; DYNAMIC ACTION;
PROTEIN-SYNTHESIS; EPISODIC HYPOXIA; CARCINUS-MAENAS; CHESAPEAKE BAY;
RESPIRATORY RESPONSES; BEHAVIORAL-RESPONSES; NEPHROPS-NORVEGICUS
AB To assess the ability of adult blue crab (Callinectes sapidus) to function under the hypoxic conditions becoming increasingly common in their inshore habitats, critical oxygen levels (i.e., the minimum oxygen levels at which aerobic metabolism can be maintained) were determined over a range of metabolic rates using automated intermittent-flow respirometry. Different metabolic rates were induced by conducting experiments at three temperatures (17, 23, and 28 degrees C), testing recently fed crabs, and those infected with the parasitic dinoflagellate Hematodinium perezi. The effects of hypoxia on the metabolic rates and recovery times of individuals following enforced exhaustive activity, and metabolic rates following feeding, were also measured to determine the levels of hypoxia likely to impact feeding, digestion, and overall energetics. Contrary to previously published results, blue crab were found not to be partial oxygen conformers (i.e., where metabolic rate falls in concert with reductions in ambient oxygen), but rather to be oxygen regulators (i.e., to have the ability to maintain a constant aerobic metabolic rate until the critical oxygen level was reached). By this measure, at routine metabolic rates blue crab are as hypoxia-tolerant as other decapod crustaceans with a median critical oxygen level of -20% air saturation (at 17 and 23 degrees C). Critical oxygen levels increased in concert with the increases in metabolic rate occurring at 28 degrees C, in individuals infected with H. perezii, and those recently fed. At the highest metabolic rates (measured in recently fed individuals at 28 degrees C) median critical oxygen level was -45% air saturation. Consistent with this latter observation, metabolic rates after feeding or exercise were not compromised until below 50% air saturation, although maximum metabolic rates were lower at this level of hypoxia. The results presented are consistent with the oxygen levels shown to influence blue crab behaviors (similar to 2 to 4 mg l(-1)) in both field and laboratory settings. Published by Elsevier B.V.
C1 [Brill, Richard W.] NOAA, James J Howard Marine Sci Lab, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Highlands, NJ USA.
[Bushnell, Peter G.] Indiana Univ, South Bend, IN 46615 USA.
[Elton, Timothy A.] Bangor Univ, Sch Ocean Sci, Menai Bridge, Gwynedd, Wales.
[Small, Hamish J.] Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA.
RP Brill, RW (reprint author), Virginia Inst Marine Sci, POB 1346, Gloucester Point, VA 23062 USA.
EM rbrill@vims.edu
FU Northeast Fisheries Science Center, National Marine Fisheries Service,
NOAA
FX We gratefully recognize J. Shields for his help in developing this
project and in diagnosing Hematodinium perezi infections, M. Coulter and
S. Johnson for their help in running the experiments, and especially the
staff of the Virginia Institute of Marine Science Eastern Shore
Laboratory for their ongoing hospitality. This is contribution 3470 from
the Virginia Institute of Marine Science. Support was provided by the
Northeast Fisheries Science Center, National Marine Fisheries Service,
NOAA. [SS]
NR 107
TC 1
Z9 1
U1 20
U2 81
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
EI 1879-1697
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD OCT
PY 2015
VL 471
BP 126
EP 136
DI 10.1016/j.jembe.2015.06.003
PG 11
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA CO4YV
UT WOS:000359167700016
ER
PT J
AU Emde, C
Barlakas, V
Cornet, C
Evans, F
Korkin, S
Ota, Y
Labonnote, LC
Lyapustin, A
Macke, A
Mayer, B
Wendisch, M
AF Emde, Claudia
Barlakas, Vasileios
Cornet, Celine
Evans, Frank
Korkin, Sergey
Ota, Yoshifumi
Labonnote, Laurent C.
Lyapustin, Alexei
Macke, Andreas
Mayer, Bernhard
Wendisch, Manfred
TI IPRT polarized radiative transfer model intercomparison project - Phase
A
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Radiative transfer; Polarization; Intercomparison; Benchmark results
ID RESEARCH SCANNING POLARIMETER; DISCRETE ORDINATE METHOD; MONTE-CARLO;
OPTICAL-PROPERTIES; SCATTERING ATMOSPHERE; PLANETARY-ATMOSPHERES;
SOFTWARE PACKAGE; SOLAR-RADIATION; AEROSOLS; CLOUDS
AB The polarization state of electromagnetic radiation scattered by atmospheric particles such as aerosols, cloud droplets, or ice crystals contains much more information about the optical and microphysical properties than the total intensity alone. For this reason an increasing number of polarimetric observations are performed from space, from the ground and from aircraft. Polarized radiative transfer models are required to interpret and analyse these measurements and to develop retrieval algorithms exploiting polarimetric observations. In the last years a large number of new codes have been developed, mostly for specific applications. Benchmark results are available for specific cases, but not for more sophisticated scenarios including polarized surface reflection and multi-layer atmospheres. The International Polarized Radiative Transfer (IPRT) working group of the International Radiation Commission (IRC) has initiated a model intercomparison project in order to fill this gap. This paper presents the results of the first phase A of the IPRT project which includes ten test cases, from simple setups with only one layer and Rayleigh scattering to rather sophisticated setups with a cloud embedded in a standard atmosphere above an ocean surface. All scenarios in the first phase A of the intercomparison project are for a one-dimensional plane-parallel model geometry. The commonly established benchmark results are available at the IPRT website (http://www.meteo.physik.uni-muenchen.de/iprt). (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Emde, Claudia; Mayer, Bernhard] Univ Munich, Inst Meteorol, Munich, Germany.
[Barlakas, Vasileios; Wendisch, Manfred] Univ Leipzig, Leipzig Inst Meteorol, D-04109 Leipzig, Germany.
[Cornet, Celine; Labonnote, Laurent C.] Univ Lille, Lab Opt Atmospher, Lille, France.
[Evans, Frank] Univ Colorado, Boulder, CO 80309 USA.
[Korkin, Sergey] Univ Space Res Assoc, Columbia, MD USA.
[Ota, Yoshifumi] Meteorol Res Inst, Tsukuba, Ibaraki 305, Japan.
[Lyapustin, Alexei] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Macke, Andreas] Leibniz Inst Tropospher Res, Leipzig, Germany.
RP Emde, C (reprint author), Univ Munich, Inst Meteorol, Theresienstr 37, Munich, Germany.
EM claudia.emde@lmu.de
RI Mayer, Bernhard/B-3397-2011; Emde, Claudia/B-5447-2010; Wendisch,
Manfred/E-4175-2013;
OI Mayer, Bernhard/0000-0002-3358-0190; Wendisch,
Manfred/0000-0002-4652-5561; EVANS, FRANK/0000-0002-5051-3176; Barlakas,
Vasileios/0000-0003-1562-4599
NR 71
TC 10
Z9 10
U1 0
U2 6
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 OCT
PY 2015
VL 164
BP 8
EP 36
DI 10.1016/j.jqsrt.2015.05.007
PG 29
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA CO9NL
UT WOS:000359502400002
ER
PT J
AU Wang, Y
AF Wang, Yuan
TI Air Pollution or Global Warming: Attribution of Extreme Precipitation
Changes in Eastern China-Comments on "Trends of Extreme Precipitation in
Eastern China and Their Possible Causes"
SO ADVANCES IN ATMOSPHERIC SCIENCES
LA English
DT Article
DE aerosol effects; global warming; extreme precipitation
ID HYDROLOGICAL CYCLE; AEROSOLS; IMPACTS; CLIMATE; CLOUDS
AB The recent study "Trends of Extreme Precipitation in Eastern China and Their Possible Causes" attributed the observed decrease/increase of light/heavy precipitation in eastern China to global warming rather than the regional aerosol effects. However, there exist compelling evidence from previous long-term observations and numerical modeling studies, suggesting that anthropogenic pollution is closely linked to the recent changes in precipitation intensity because of considerably modulated cloud physical properties by aerosols in eastern China. Clearly, a quantitative assessment of the aerosol and greenhouse effects on the regional scale is required to identify the primary cause for the extreme precipitation changes.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wang, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM yuan.wang@jpl.nasa.gov
FU National Aeronautics and Space Administration [ROSES14-ACMAP]
FX The author appreciates the funding support provided by the National
Aeronautics and Space Administration (Grant No. ROSES14-ACMAP).
NR 21
TC 3
Z9 3
U1 12
U2 68
PU SCIENCE PRESS
PI BEIJING
PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA
SN 0256-1530
EI 1861-9533
J9 ADV ATMOS SCI
JI Adv. Atmos. Sci.
PD OCT
PY 2015
VL 32
IS 10
BP 1444
EP 1446
DI 10.1007/s00376-015-5109-4
PG 3
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CO2UK
UT WOS:000359011900011
ER
PT J
AU Miki, K
Panesi, M
Prudhomme, S
AF Miki, Kenji
Panesi, Marco
Prudhomme, Serge
TI Systematic validation of non-equilibrium thermochemical models using
Bayesian inference
SO JOURNAL OF COMPUTATIONAL PHYSICS
LA English
DT Article
DE Parameter identification; Inverse problem; Nitrogen ionization; Bayesian
inference; Covariance matrix; Stochastic modeling
ID UNCERTAINTY QUANTIFICATION; DISSOCIATION; NITROGEN
AB The validation process proposed by Babuska etal. [1] is applied to thermochemical models describing post-shock flow conditions. In this validation approach, experimental data is involved only in the calibration of the models, and the decision process is based on quantities of interest (QoIs) predicted on scenarios that are not necessarily amenable experimentally. Moreover, uncertainties present in the experimental data, as well as those resulting from an incomplete physical model description, are propagated to the QoIs. We investigate four commonly used thermochemical models: a one-temperature model (which assumes thermal equilibrium among all inner modes), and two-temperature models developed by Macheret etal. [2], Marrone and Treanor [3], and Park [4]. Up to 16 uncertain parameters are estimated using Bayesian updating based on the latest absolute volumetric radiance data collected at the Electric Arc Shock Tube (EAST) installed inside the NASA Ames Research Center. Following the solution of the inverse problems, the forward problems are solved in order to predict the radiative heat flux, QoI, and examine the validity of these models. Our results show that all four models are invalid, but for different reasons: the one-temperature model simply fails to reproduce the data while the two-temperature models exhibit unacceptably large uncertainties in the QoI predictions. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Miki, Kenji] NASA, Glenn Res Ctr, Cleveland, OH 44142 USA.
[Panesi, Marco] Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.
[Prudhomme, Serge] Ecole Polytech, Dept Math & Genie Ind, Montreal, PQ H3C 3A7, Canada.
RP Panesi, M (reprint author), Univ Illinois, Dept Aerosp Engn, 306 Talbot Lab,104 S Wright St, Urbana, IL 61801 USA.
EM mpanesi@illinois.edu
NR 47
TC 0
Z9 0
U1 6
U2 7
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0021-9991
EI 1090-2716
J9 J COMPUT PHYS
JI J. Comput. Phys.
PD OCT 1
PY 2015
VL 298
BP 125
EP 144
DI 10.1016/j.jcp.2015.05.011
PG 20
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA CN9UY
UT WOS:000358796700008
ER
PT J
AU Chiachio, J
Chiachio, M
Sankararaman, S
Saxena, A
Goebel, K
AF Chiachio, Juan
Chiachio, Manuel
Sankararaman, Shankar
Saxena, Abhinav
Goebel, Kai
TI Condition-based prediction of time-dependent reliability in composites
SO RELIABILITY ENGINEERING & SYSTEM SAFETY
LA English
DT Article
DE Model-based prognostics; Time-dependent reliability; Fatigue; Composites
ID FATIGUE DAMAGE PROGNOSIS; MODEL-BASED PROGNOSTICS; VARIATIONAL APPROACH;
UNCERTAINTY; CRACKS; REDUCTION; FRACTURE
AB This paper presents a reliability-based prediction methodology to obtain the remaining useful life of composite materials subjected to fatigue degradation. Degradation phenomena such as stiffness reduction and increase in matrix micro-cracks density are sequentially estimated through a Bayesian filtering framework that incorporates information from both multi-scale damage models and damage measurements, that are sequentially collected along the process. A set of damage states are further propagated forward in time by simulating the damage progression using the models in the absence of new damage measurements to estimate the time-dependent reliability of the composite material. As a key contribution, the estimation of the remaining useful life is obtained as a probability from the prediction of the time-dependent reliability, whose validity is formally proven using the axioms of Probability Logic. A case study is presented using multi-scale fatigue damage data from a cross-ply carbon-epoxy laminate. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Chiachio, Juan; Chiachio, Manuel] Univ Granada, Dept Struct Mech & Hydraul Engn, E-18071 Granada, Spain.
[Sankararaman, Shankar; Saxena, Abhinav] NASA, Ames Res Ctr, SGT Inc, Moffett Field, CA 94035 USA.
[Goebel, Kai] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
RP Chiachio, J (reprint author), ETS Ingenieros Caminos Canales & Puertos, Campus Fuentenueva S-N, Granada 18071, Spain.
EM jchiachio@ugr.es
OI CHIACHIO, JUAN/0000-0003-1243-8694
FU Ministry of Education of Spain [AP2009-4641, AP2009-2390]; Prognostics
Center of Excellence at NASA Ames Research Center; NASA ARMD/AvSafe
project SSAT
FX The two first authors would like to thank the Ministry of Education of
Spain for the FPU grants AP2009-4641, AP2009-2390 and the Prognostics
Center of Excellence at NASA Ames Research Center, which kindly hosted
them during the course of this work. Authors would also like to thank
the Structures and Composites lab at Stanford University for
experimental data and NASA ARMD/AvSafe project SSAT, which provided
partial support for this work.
NR 60
TC 12
Z9 12
U1 5
U2 20
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0951-8320
EI 1879-0836
J9 RELIAB ENG SYST SAFE
JI Reliab. Eng. Syst. Saf.
PD OCT
PY 2015
VL 142
BP 134
EP 147
DI 10.1016/j.ress.2015.04.018
PG 14
WC Engineering, Industrial; Operations Research & Management Science
SC Engineering; Operations Research & Management Science
GA CO5AQ
UT WOS:000359172400014
ER
PT J
AU Geogdzhayev, IV
Mishchenko, MI
Li, J
Rossow, WB
Liu, L
Cairns, B
AF Geogdzhayev, Igor V.
Mishchenko, Michael I.
Li, Jing
Rossow, William B.
Liu, Li
Cairns, Brian
TI Extension and statistical analysis of the GACP aerosol optical thickness
record
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Tropospheric aerosols; Aerosol remote sensing; Optical thickness; Global
Aerosol Climatology Project; Long-term trends; Principal Component
Analysis
ID COMPARE SPATIOTEMPORAL VARIABILITY; SPECTRAL-ANALYSIS TECHNIQUES; AVHRR
RADIANCES; CHANNELS 1; SATELLITE; CALIBRATION; RETRIEVALS; MODIS;
TRENDS; OCEAN
AB The primary product of the Global Aerosol Climatology Project (GACP) is a continuous record of the aerosol optical thickness (AOT) over the oceans. It is based on channel-1 and -2 radiance data from the Advanced Very High Resolution Radiometer (AVHRR) instruments flown on successive National Oceanic and Atmospheric Administration (NOAA) platforms. We extend the previous GACP dataset by four years through the end of 2009 using NOAA-17 and -18 AVHRR radiances recalibrated against MODerate resolution Imaging Spectroradiometer (MODIS) radiance data, thereby making the GACP record almost three decades long. The temporal overlap of over three years of the new NOAA-17 and the previous NOAA-16 record reveals an excellent agreement of the corresponding global monthly mean AOT values, thereby confirming the robustness of the vicarious radiance calibration used in the original GACP product. The temporal overlap of the NOAA-17 and -18 instruments is used to introduce a small additive adjustment to the channel-2 calibration of the latter resulting in a consistent record with increased data density. The Principal Component Analysis (PCA) of the newly extended GACP record shows that most of the volcanic AOT variability can be isolated into one mode responsible for similar to 12% of the total variance. This conclusion is confirmed by a combined PCA analysis of the GACP, MODIS, and Multi-angle Imaging SpectroRadiometer (MISR) AOTs during the volcano-free period from February 2000 to December 2009. We show that the modes responsible for the tropospheric AOT variability in the three datasets agree well in terms of correlation and spatial patterns. A previously identified negative AOT trend which started in the late 1980s and continued into the early 2000s is confirmed. Its magnitude and duration indicate that it was caused by changes in tropospheric aerosols. The latest multi-satellite segment of the GACP record shows that this trend tapered off, with no noticeable AOT change after 2002. This result is consistent with the MODIS and MISR AOT records as well as with the recent gradual reversal from brightening to dimming revealed by surface flux measurements in many aerosol producing regions. Thus the robustness of the GACP record is confirmed, increasing our confidence in the validity of the negative trend. Although the nominal negative GACP AOT trend could partially be an artifact of increasing aerosol absorption, we argue that the time dependence of the GACP record, including the latest flat period, is more consistent with the actual decrease in the tropospheric AOT. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Geogdzhayev, Igor V.; Li, Jing; Liu, Li] Columbia Univ, New York, NY 10025 USA.
[Geogdzhayev, Igor V.; Mishchenko, Michael I.; Li, Jing; Liu, Li; Cairns, Brian] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Li, Jing] Scripps Inst Oceanog, La Jolla, CA 92037 USA.
[Rossow, William B.] CUNY City Coll, Dept Elect Engn, New York, NY 10031 USA.
RP Geogdzhayev, IV (reprint author), Columbia Univ, 2880 Broadway, New York, NY 10025 USA.
EM igor.v.geogdzhayev@nasa.gov
OI Cairns, Brian/0000-0002-1980-1022
FU NASA Radiation Sciences Program
FX We thank two anonymous reviewers for insightful comments that have
resulted in a much improved manuscript. This research was supported by
the NASA Radiation Sciences Program managed by Hal Maring.
NR 59
TC 2
Z9 2
U1 0
U2 4
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD OCT 1
PY 2015
VL 164
BP 268
EP 277
DI 10.1016/j.atmosres.2015.05.013
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CN0HX
UT WOS:000358095800022
ER
PT J
AU Kugler, F
Lee, SK
Hajnsek, I
Papathanassiou, KP
AF Kugler, Florian
Lee, Seung-Kuk
Hajnsek, Irena
Papathanassiou, Konstantinos P.
TI Forest Height Estimation by Means of Pol-InSAR Data Inversion: The Role
of the Vertical Wavenumber
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Forest height; L-band; P-band; polarimetric synthetic aperture radar
interferometry (Pol-InSAR); spatial baseline; terrain slope
ID POLARIMETRIC SAR INTERFEROMETRY; SYNTHETIC-APERTURE RADAR; TEMPORAL
DECORRELATION; BOREAL FOREST; L-BAND; PARAMETER-ESTIMATION; VEGETATION
STRUCTURE; TANDEM-X; LIDAR; RESOLUTION
AB This paper examines the multifaceted effect of the effective spatial baseline, as expressed through the vertical (interferometric) wavenumber, on the inversion of forest height from polarimetric interferometric synthetic aperture radar (Pol-InSAR) data. First, the role of the vertical wavenumber in relating forest height to the interferometric (volume) coherence is introduced. Through the review of the forest height inversion from Pol-InSAR data, the effect of the vertical wavenumber on the inversion performance is evaluated. The selection of optimum with respect to forest height inversion performance, vertical wavenumbers is discussed. The impact of the acquisition geometry and terrain slopes on the vertical wavenumber and their consideration in the inversion methodology is addressed. The individual effects discussed are demonstrated by means of airborne repeat pass Pol-InSAR acquisitions in L- and P-band acquired over different forest conditions, including a boreal, a temperate, and a tropical forest test site. The achieved forest height inversion performance is validated against reference height data derived from airborne LIDAR acquisitions.
C1 [Kugler, Florian; Papathanassiou, Konstantinos P.] German Aerosp Ctr, Microwaves & Radar Inst, D-82234 Oberpfaffenhofen, Germany.
[Lee, Seung-Kuk] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hajnsek, Irena] Swiss Fed Inst Technol, Inst Umweltingenieurwissenschaf, CH-8093 Zurich, Switzerland.
[Hajnsek, Irena] German Aerosp Ctr DLR HR, Microwaves & Radar Inst, D-82234 Oberpfaffenhofen, Germany.
RP Kugler, F (reprint author), German Aerosp Ctr, Microwaves & Radar Inst, D-82234 Oberpfaffenhofen, Germany.
EM florian.kugler@dlr.de; seungkuk.lee@nasa.gov; irena.hajnsek@dlr.de;
kostas.papathanassiou@dlr.de
FU HGF Helmholtz Alliance; ESA's BioSAR II campaign [22052/08/NL/CT]
FX This work was supported in part by the HGF Helmholtz Alliance "Remote
Sensing & Earth System Dynamics." Krycklan data were acquired in the
frame of ESA's BioSAR II campaign under Contract 22052/08/NL/CT).
NR 81
TC 13
Z9 13
U1 3
U2 20
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 OCT
PY 2015
VL 53
IS 10
BP 5294
EP 5311
DI 10.1109/TGRS.2015.2420996
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 CK4AQ
UT WOS:000356159900002
ER
PT J
AU Wang, ZP
Xiong, XX
Li, YH
AF Wang, Zhipeng
Xiong, Xiaoxiong
Li, Yonghong
TI Update of VIIRS On-Orbit Spatial Parameters Characterized With the Moon
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Band-to-band registration (BBR); detector-to-detector registration
(DDR); lunar calibration; modulation transfer function (MTF); spatial
characterization; Visible Infrared Imaging Radiometer Suite (VIIRS)
ID PERFORMANCE
AB The Visible Infrared Imaging Radiometer Suite (VIIRS) instrument aboard the Suomi National Polar-orbiting Partnership satellite has been successfully operating since its launch on October 28, 2011. Unlike its predecessor MODerate resolution Imaging Spectroradiometer (MODIS), VIIRS has no independent onboard calibrator to perform the on-orbit characterization of its spatial parameters such as the band-to-band registration (BBR), detector-to-detector registration (DDR), and modulation transfer function (MTF). The surface properties of the Moon have been demonstrated to be spectrally, radiometrically, and geometrically stable in the long term, making the Moon a suitable target for the on-orbit calibration of satelliteborne remote sensing instruments. The methodologies of spatial characterization using the Moon have been developed for MODIS and validated, through the comparison of their results to those calibrated by the onboard spatial calibrator of MODIS. In this paper, the methodologies are extended and improved for VIIRS applications. The BBR, DDR in both along-scan and along-track directions and the MTF in the along-track direction of VIIRS are calculated from the lunar observations scheduled on a nearly monthly basis. The trending results confirm that these parameters have been stable over time: the BBR offset is less than 0.05 pixels in both directions, well within the performance specification requirement of 0.1 pixels. The along-track MTF is approximately 0.6, well above the specification of 0.3, and is consistent with the prelaunch measurement. The limitation of the current methodologies and the possible future improvements are also discussed in this paper.
C1 [Wang, Zhipeng; Li, Yonghong] Sci Syst & Applicat Inc, Greenbelt, MD 20706 USA.
[Xiong, Xiaoxiong] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wang, ZP (reprint author), Sci Syst & Applicat Inc, Greenbelt, MD 20706 USA.
EM zhipeng.wang@ssaihq.com; XiaoxiongXiong-1@nasa.gov;
yonghong.li@ssaihq.com
OI Wang, Zhipeng/0000-0002-9108-9009
NR 20
TC 2
Z9 2
U1 2
U2 6
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 OCT
PY 2015
VL 53
IS 10
BP 5486
EP 5494
DI 10.1109/TGRS.2015.2423633
PG 9
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA CK4AQ
UT WOS:000356159900015
ER
PT J
AU Basu, S
Ganguly, S
Nemani, RR
Mukhopadhyay, S
Zhang, G
Milesi, C
Michaelis, A
Votava, P
Dubayah, R
Duncanson, L
Cook, B
Yu, YF
Saatchi, S
DiBiano, R
Karki, M
Boyda, E
Kumar, U
Li, S
AF Basu, Saikat
Ganguly, Sangram
Nemani, Ramakrishna R.
Mukhopadhyay, Supratik
Zhang, Gong
Milesi, Cristina
Michaelis, Andrew
Votava, Petr
Dubayah, Ralph
Duncanson, Laura
Cook, Bruce
Yu, Yifan
Saatchi, Sassan
DiBiano, Robert
Karki, Manohar
Boyda, Edward
Kumar, Uttam
Li, Shuang
TI A Semiautomated Probabilistic Framework for Tree-Cover Delineation From
1-m NAIP Imagery Using a High-Performance Computing Architecture
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aerial imagery; conditional random field (CRF); high-performance
computing (HPC); machine learning; National Agriculture Imagery Program
(NAIP); neural network (NN); statistical region merging (SRM)
ID LAND-COVER; AUTOMATIC DETECTION; CLASSIFICATION; CROWN; SEGMENTATION;
VEGETATION; ALGORITHM; MODIS; CUTS
AB Accurate tree-cover estimates are useful in deriving above-ground biomass density estimates from very high resolution (VHR) satellite imagery data. Numerous algorithms have been designed to perform tree-cover delineation in high-to-coarse-resolution satellite imagery, but most of them do not scale to terabytes of data, typical in these VHR data sets. In this paper, we present an automated probabilistic framework for the segmentation and classification of 1-m VHR data as obtained from the National Agriculture Imagery Program (NAIP) for deriving tree-cover estimates for the whole of Continental United States, using a high-performance computing architecture. The results from the classification and segmentation algorithms are then consolidated into a structured prediction framework using a discriminative undirected probabilistic graphical model based on conditional random field, which helps in capturing the higher order contextual dependence relations between neighboring pixels. Once the final probability maps are generated, the framework is updated and retrained by incorporating expert knowledge through the relabeling of misclassified image patches. This leads to a significant improvement in the true positive rates and reduction in false positive rates (FPRs). The tree-cover maps were generated for the state of California, which covers a total of 11 095 NAIP tiles and spans a total geographical area of 163 696 sq. miles. Our framework produced correct detection rates of around 88% for fragmented forests and 74% for urban tree-cover areas, with FPRs lower than 2% for both regions. Comparative studies with the National Land-Cover Data algorithm and the LiDAR high-resolution canopy height model showed the effectiveness of our algorithm for generating accurate high-resolution tree-cover maps.
C1 [Basu, Saikat; Mukhopadhyay, Supratik; DiBiano, Robert; Karki, Manohar] Louisiana State Univ, Dept Comp Sci, Baton Rouge, LA 70803 USA.
[Ganguly, Sangram; Zhang, Gong] NASA Ames Res Ctr, BAERI, Moffett Field, CA 94035 USA.
[Nemani, Ramakrishna R.] NASA Ames Res Ctr, NASA Adv Supercomp Div, Moffett Field, CA 94035 USA.
[Milesi, Cristina] NASA Ames Res Ctr, Biospher Sci Branch, Moffett Field, CA 94035 USA.
[Michaelis, Andrew; Votava, Petr; Li, Shuang] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Michaelis, Andrew; Votava, Petr; Li, Shuang] Univ Corp Monterey, Moffett Field, CA 94035 USA.
[Dubayah, Ralph; Duncanson, Laura] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Cook, Bruce] NASA Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Yu, Yifan] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Boyda, Edward] St Marys Coll Calif, Dept Phys & Astron, Moraga, CA 94575 USA.
[Kumar, Uttam] Oak Ridge Associated Univ, NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Basu, S (reprint author), Louisiana State Univ, Dept Comp Sci, Baton Rouge, LA 70803 USA.
EM sbasu8@lsu.edu
FU NASA Carbon Monitoring System [NNH14ZDA001-N-CMS]; CFDA [43.001];
[NASA-NNX12AD05A]
FX This work was supported in part by the NASA Carbon Monitoring System
under Grant NNH14ZDA001-N-CMS and in part by the Cooperative Agreement
NASA-NNX12AD05A, CFDA Number 43.001, through the project identified as
"Ames Research Center Cooperative for Research in Earth Science and
Technology (ARC-CREST)."
NR 47
TC 1
Z9 1
U1 5
U2 32
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 OCT
PY 2015
VL 53
IS 10
BP 5690
EP 5708
DI 10.1109/TGRS.2015.2428197
PG 19
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA CK4AQ
UT WOS:000356159900031
ER
PT J
AU Xiong, XX
Wu, AS
Wenny, BN
Madhavan, S
Wang, ZP
Li, YH
Chen, N
Barnes, WL
Salomonson, VV
AF Xiong, Xiaoxiong
Wu, Aisheng
Wenny, Brian N.
Madhavan, Sriharsha
Wang, Zhipeng
Li, Yonghong
Chen, Na
Barnes, William L.
Salomonson, Vincent V.
TI Terra and Aqua MODIS Thermal Emissive Bands On-Orbit Calibration and
Performance
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aqua; blackbody (BB); calibration; detector; Moderate Resolution Imaging
Spectroradiometer (MODIS); Terra; thermal emissive bands (TEBs);
uncertainty
ID IMAGING SPECTRORADIOMETER MODIS; LESSONS
AB Since launch, the Moderate Resolution Imaging Spectroradiometer (MODIS) instruments on the Terra and Aqua spacecraft have operated successfully for more than 14 and 12 years, respectively. A key instrument for National Aeronautics and Space Administration Earth Observing System missions, MODIS was designed to make continuous observations for studies of Earth's land, ocean, and atmospheric properties and to extend existing data records from heritage Earth observing sensors. The 16 thermal emissive bands (TEBs) (3.75-14.24 mu m) are calibrated on orbit using a temperature controlled blackbody (BB). Both Terra and Aqua MODIS BBs have displayed minimal drift over the mission lifetime, and the seasonal variations of the BB temperature are extremely small in Aqua MODIS. The long-term gain and noise equivalent difference in temperature performance of the 160 TEB detectors on both MODIS instruments have been well behaved and generally very stable. Small but noticeable variations of Aqua MODIS bands 33-36 (13.34-14.24 mu m) response in recent years are primarily due to loss of temperature control margin of its passive cryoradiative cooler. As a result, fixed calibration coefficients, previously used by bands when the BB temperature is above their saturation temperatures, are replaced by the focal-plane-temperature-dependent calibration coefficients. This paper presents an overview of the MODIS TEB calibration, the on-orbit performance, and the challenging issues likely to impact the instruments as they continue operating well past their designed lifetime of six years.
C1 [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Wu, Aisheng; Wenny, Brian N.; Madhavan, Sriharsha; Wang, Zhipeng; Li, Yonghong; Chen, Na] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Barnes, William L.] Univ Maryland, Baltimore, MD 21250 USA.
[Salomonson, Vincent V.] Univ Utah, Salt Lake City, UT 84112 USA.
[Salomonson, Vincent V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Xiong, XX (reprint author), NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
EM Xiaoxiong.Xiong-1@nasa.gov; aisheng.wu@ssaihq.com;
brian.wenny@ssaihq.com; sriharsha.madhavan@ssaihq.com;
zhipeng.wang@ssaihq.com; yonghong.li@ssaihq.com; Na.Chen@ssaihq.com;
wlbarnes9@satx.rr.com; vincent.v.salomonson@nasa.gov
OI Wang, Zhipeng/0000-0002-9108-9009
NR 24
TC 17
Z9 17
U1 0
U2 7
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 OCT
PY 2015
VL 53
IS 10
BP 5709
EP 5721
DI 10.1109/TGRS.2015.2428198
PG 13
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA CK4AQ
UT WOS:000356159900032
ER
PT J
AU Sun, JQ
Madhavan, S
Xiong, XX
Wang, MH
AF Sun, Junqiang
Madhavan, Sriharsha
Xiong, Xiaoxiong
Wang, Menghua
TI Investigation of the Electronic Crosstalk in Terra MODIS Band 28
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Crosstalk; Moderate Resolution Imaging Spectroradiometer (MODIS); moon;
radiometric improvements; striping; Terra; thermal emissive bands (TEBs)
ID THERMAL EMISSIVE BANDS; REFLECTIVE SOLAR BANDS; CALIBRATION;
PERFORMANCE; AQUA
AB The Moderate Resolution Imaging Spectroradiometer (MODIS) is a whisk broom scanning radiometer, which is onboard the Terra and Aqua spacecraft. Both MODIS instruments have successfully completed more than 12 years of on-orbit flight. The long-wave infrared (LWIR) photovoltaic bands (bands 27-30, 6.72-9.73 mu m) on the LWIR focal plane assembly in Terra MODIS have contamination due to electronic crosstalk. In this paper, we examine Terra MODIS band 28 (7.33 mu m) crosstalk effects, their impact, and mitigation. The crosstalk signal is identified and characterized using the regular lunar observations acquired by MODIS. It is evident from the derived crosstalk coefficients that the contamination was mainly from bands 27 (6.72 mu m), 29 (8.55 mu m), and 30 (9.73 mu m). The crosstalk coefficients are generally a small positive quantity in the early to middle part of the mission with a few exceptions, and then changing directions. A linear correction algorithm is applied to both L1B calibration and retrieval to qualitatively and quantitatively assess the impact and improvements in this paper. It is shown that the crosstalk correction improved the imagery and radiometric fidelity of this band.
C1 [Sun, Junqiang; Wang, Menghua] NOAA Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, College Pk, MD 20740 USA.
[Sun, Junqiang] Global Sci & Technol, Greenbelt, MD 20770 USA.
[Madhavan, Sriharsha] Sci & Syst Applicat Inc, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong] NASA Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
RP Sun, JQ (reprint author), NOAA Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, College Pk, MD 20740 USA.
EM junqiang.sun@noaa.gov; sriharsha.madhavan@ssaihq.com;
Xiaoxiong.Xiong-1@nasa.gov; menghua.wang@noaa.gov
RI Wang, Menghua/F-5631-2010
OI Wang, Menghua/0000-0001-7019-3125
NR 18
TC 9
Z9 9
U1 0
U2 2
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 OCT
PY 2015
VL 53
IS 10
BP 5722
EP 5733
DI 10.1109/TGRS.2015.2428212
PG 12
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA CK4AQ
UT WOS:000356159900033
ER
PT J
AU Han, JW
Rim, T
Baek, CK
Meyyappan, M
AF Han, Jin-Woo
Rim, Taiuk
Baek, Chang-Ki
Meyyappan, M.
TI Chemical Gated Field Effect Transistor by Hybrid Integration of
One-Dimensional Silicon Nanowire and Two-Dimensional Tin Oxide Thin Film
for Low Power Gas Sensor
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE gas sensor; field effect transistor; nanowire; thin film; tin oxide
ID FET SENSORS; DEVICES; ARRAYS; O-2; NO2; CO
AB Gas sensors based on metal-oxide-semiconductor transistor with the polysilicon gate replaced by a gas sensitive thin film have been around for over SO years. These are not suitable for the emerging mobile and wearable sensor platforms due to operating voltages and powers far exceeding the supply capability of batteries. Here we present a novel approach to decouple the chemically sensitive region from the conducting channel for reducing the drive voltage and increasing reliability. This chemically gated field effect transistor uses silicon nanowire for the current conduction channel with a tin oxide film on top of the nanowire serving as the gas sensitive medium. The potential change induced by the molecular adsorption and desorption allows the electrically floating tin oxide film to gate the silicon channel. As the device is designed to be normally off, the power is consumed only during the gas sensing event. This feature is attractive for the battery operated sensor and wearable electronics. In addition, the decoupling of the chemical reaction and the current conduction regions allows the gas sensitive material to be free from electrical stress, thus increasing reliability. The device shows excellent gas sensitivity to the tested analytes relative to conventional metal oxide transistors and resistive sensors.
C1 [Han, Jin-Woo; Meyyappan, M.] NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rim, Taiuk; Baek, Chang-Ki] Pohang Univ Sci & Technol, Creat IT Engn, Pohang 790784, South Korea.
RP Han, JW (reprint author), NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jin-woo.han@nasa.gov
FU IT Consilience Creative Program [NIPA-2014-H0201-14-1001]; NASA
[NNX12AK33A]
FX This work was supported by the "IT Consilience Creative Program"
(NIPA-2014-H0201-14-1001) supervised by the National IT Industry
Promotion Agency, Korea. J.W.H. is with USRA, and the material is based
upon work supported by NASA under award NNX12AK33A.
NR 31
TC 4
Z9 4
U1 11
U2 71
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1944-8244
J9 ACS APPL MATER INTER
JI ACS Appl. Mater. Interfaces
PD SEP 30
PY 2015
VL 7
IS 38
BP 21263
EP 21269
DI 10.1021/acsami.5b05479
PG 7
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA CS7DE
UT WOS:000362243500031
PM 26381613
ER
PT J
AU Shen, ZZ
Szlufarska, I
Brown, PE
Xu, HF
AF Shen, Zhizhang
Szlufarska, Izabela
Brown, Philip E.
Xu, Huifang
TI Investigation of the Role of Polysaccharide in the Dolomite Growth at
Low Temperature by Using Atomistic Simulations
SO LANGMUIR
LA English
DT Article
ID SULFATE-REDUCING BACTERIA; CALCITE-WATER INTERFACE; FREE-ENERGY;
(104)-WATER INTERFACE; SEDIMENTARY DOLOMITE; DISORDERED DOLOMITE;
FORCE-FIELD; PRECIPITATION; SURFACE; DOLOMITIZATION
AB Dehydration of water from surface Mg2+ is most likely the rate-limiting step in the dolomite growth at low temperature. Here, we investigate the role of polysaccharide in this step using classical molecular dynamics (MD) calculations. Free energy (potential of mean force, PMF) calculations have been performed for water molecules leaving the first two hydration layers above the dolomite (104) surface under the following three conditions: without catalyst, with monosaccharide (mannose), and with oligosaccharide (three units of mannose). MD simulations reveal that there is no obvious effect of monosaccharide in lowering the dehydration barrier for surface Mg2+. However, we found that there are metastable configurations of oligosaccharide, which can decrease the dehydration barrier of surface Mg2+ by about 0.7-1.1 kcal/mol. In these configurations, the molecule lies relatively flat on the surface and forms a bridge shape. The hydrophobic space near the surface created by the nonpolar -CH groups of the oligosaccharide in the bridge conformation is the reason for the observed reduction of dehydration barrier.
C1 [Shen, Zhizhang; Brown, Philip E.; Xu, Huifang] Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA.
[Szlufarska, Izabela] Univ Wisconsin, Dept Mat Sci & Engn, Madison, WI 53706 USA.
[Szlufarska, Izabela; Xu, Huifang] Univ Wisconsin, Mat Sci Program, Madison, WI 53706 USA.
RP Szlufarska, I (reprint author), Univ Wisconsin, Dept Mat Sci & Engn, 1509 Univ Ave, Madison, WI 53706 USA.
EM szlufarska@wisc.edu; hfxu@geology.wisc.edu
FU NSF [EAR-095800, EAR-0910779]; NASA Astrobiology Institute [N07-5489];
Department of Geoscience
FX Zhizhang Shen and Huifang Xu acknowledge supports from NSF (EAR-095800)
and NASA Astrobiology Institute (N07-5489). Izabela Szlufarska
acknowledges support from NSF (EAR-0910779). Zhizhang Shen also thanks
S. W. Bailey Distinguished Graduate Fellowship of the Department of
Geoscience for supporting his research.
NR 45
TC 1
Z9 1
U1 3
U2 13
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0743-7463
J9 LANGMUIR
JI Langmuir
PD SEP 29
PY 2015
VL 31
IS 38
BP 10435
EP 10442
DI 10.1021/acs.langmuir.5b02025
PG 8
WC Chemistry, Multidisciplinary; Chemistry, Physical; Materials Science,
Multidisciplinary
SC Chemistry; Materials Science
GA CS7DF
UT WOS:000362243600014
PM 26334253
ER
PT J
AU Liao, YL
Tu, KX
Han, XG
Hu, LB
Connell, JW
Chen, ZF
Lin, Y
AF Liao, Yunlong
Tu, Kaixiong
Han, Xiaogang
Hu, Liangbing
Connell, John W.
Chen, Zhongfang
Lin, Yi
TI Oxidative Etching of Hexagonal Boron Nitride Toward Nanosheets with
Defined Edges and Holes
SO SCIENTIFIC REPORTS
LA English
DT Article
ID POROUS GRAPHENE MATERIALS; ENERGY-STORAGE; BULK PREPARATION; NANOMESH;
NANORIBBONS; NANOTUBES; VAPOR; FABRICATION; GROWTH; OXIDE
AB Lateral surface etching of two-dimensional (2D) nanosheets results in holey 2D nanosheets that have abundant edge atoms. Recent reports on holey graphene showed that holey 2D nanosheets can outperform their intact counterparts in many potential applications such as energy storage, catalysis, sensing, transistors, and molecular transport/separation. From both fundamental and application perspectives, it is desirable to obtain holey 2D nanosheets with defined hole morphology and hole edge structures. This remains a great challenge for graphene and is little explored for other 2D nanomaterials. Here, a facile, controllable, and scalable method is reported to carve geometrically defined pit/hole shapes and edges on hexagonal boron nitride (h-BN) basal plane surfaces via oxidative etching in air using silver nanoparticles as catalysts. The etched h-BN was further purified and exfoliated into nanosheets that inherited the hole/edge structural motifs and, under certain conditions, possess altered optical bandgap properties likely induced by the enriched zigzag edge atoms. This method opens up an exciting approach to further explore the physical and chemical properties of hole-and edge-enriched boron nitride and other 2D nanosheets, paving the way toward applications that can take advantage of their unique structures and performance characteristics.
C1 [Liao, Yunlong; Lin, Yi] NIA, Hampton, VA 23666 USA.
[Liao, Yunlong; Tu, Kaixiong; Chen, Zhongfang] Univ Puerto Rico, Inst Funct Nanomat, Dept Chem, San Juan, PR 00931 USA.
[Han, Xiaogang; Hu, Liangbing] Univ Maryland, Dept Mat Sci & Engn, College Pk, MD 20742 USA.
[Connell, John W.] NASA Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
[Lin, Yi] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23185 USA.
RP Chen, ZF (reprint author), Univ Puerto Rico, Inst Funct Nanomat, Dept Chem, Rio Piedras Campus, San Juan, PR 00931 USA.
EM zhongfangchen@gmail.com; yi.lin@nianet.org
RI Chen, Zhongfang/A-3397-2008; Hu, Liangbing/N-6660-2013
FU Institute for Functional Nanomaterials (IFN) at University of Puerto
Rico; National Institute of Aerospace; Internal Research and Development
(IRAD) program from NASA Langley Research Center; Department of Defense
[W911NF-12-1-0083]; NASA [NNX10AM80H, NNX13AB22A]
FX The authors thank Dr. W. Cao and Prof. H. Elsayed-Ali at Applied
Research Center of Old Dominion University for their experimental
assistance in acquiring HR-TEM images and C. Chamberlain at NASA Langley
Research Center in conducting TGA experiments. Y. Liao is partially
supported by the fellowship awarded via Institute for Functional
Nanomaterials (IFN) at University of Puerto Rico. Y. Lin acknowledges
the financial support by National Institute of Aerospace and the
Internal Research and Development (IRAD) program from NASA Langley
Research Center. Z. Chen acknowledges the support by Department of
Defense (Grant W911NF-12-1-0083) and NASA (Grant Nos. NNX10AM80H and
NNX13AB22A).
NR 37
TC 9
Z9 9
U1 24
U2 115
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD SEP 29
PY 2015
VL 5
AR 14510
DI 10.1038/srep14510
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CS2DT
UT WOS:000361878700001
PM 26416484
ER
PT J
AU Ooijevaar, TH
Rogge, MD
Loendersloot, R
Warnet, LL
Akkerman, R
Tinga, T
AF Ooijevaar, T. H.
Rogge, M. D.
Loendersloot, R.
Warnet, L. L.
Akkerman, R.
Tinga, T.
TI Nonlinear dynamic behavior of an impact damaged composite skin-stiffener
structure
SO JOURNAL OF SOUND AND VIBRATION
LA English
DT Article
ID ELASTIC-WAVE SPECTROSCOPY; DISCERN MATERIAL DAMAGE; ACOUSTIC
NONLINEARITY; PARAMETER-ESTIMATION; NEWS TECHNIQUES; VIBRATION
AB One of the key issues in composite structures for aircraft applications is the early identification of damage. Often, service induced damage does not involve visible plastic deformation, but internal matrix related damage. A wide range of technologies, comprising global vibration and local wave propagation methods, can be employed for health monitoring purposes. Traditional modal analysis based methods are linear methods. The effectiveness of these methods is sometimes limited since they rely on a stationary and linear description of the system. The nonlinear interaction between a low frequency wave Field and a local impact induced damage in a composite skin-stiffener structure is experimentally demonstrated in this work. The different mechanisms linked to the distorted waveforms are separated with the help of phase portraits. The harmonic waveform distortions are concentrated at the damaged region and increased for higher excitation amplitudes. It is shown that linear damage identification methods are feasible for low excitation amplitudes, but that the presence of nonlinear dynamic effects cannot remain silent for higher amplitudes. Analyzing the damage induced nonlinear effects can provide useful information about the current state of the structure. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Ooijevaar, T. H.; Warnet, L. L.; Akkerman, R.] Univ Twente, Fac Engn Technol Prod Technol, NL-7500 AE Enschede, Netherlands.
[Rogge, M. D.] NASA, Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23665 USA.
[Ooijevaar, T. H.; Loendersloot, R.; Tinga, T.] Univ Twente, Fac Engn Technol dynam Based Maintenance, NL-7500 AE Enschede, Netherlands.
RP Ooijevaar, TH (reprint author), Univ Twente, Fac Engn Technol, POB 217, NL-7500 AE Enschede, Netherlands.
EM ted@dvonline.net
FU National Aeronautics and Space Administration Langley Research Center
[NNL09AA00A]; Fokker Aerostructures B.V., Hoogeveen, The Netherlands;
European research project Clean Sky, Eco-Design Integrated Technology
Demonstrator [CSJU-GAM-ED-2008-001]
FX This material is based on work supported by National Aeronautics and
Space Administration Langley Research Center under Research Cooperative
Agreement no. NNL09AA00A awarded to the National Institute of
Aerospace.; The authors kindly acknowledge the support of Fokker
Aerostructures B.V., Hoogeveen, The Netherlands, for manufacturing the
composite structure used in this research. This work is funded by the
European research project Clean Sky, Eco-Design Integrated Technology
Demonstrator (Grant agreement number CSJU-GAM-ED-2008-001).
NR 23
TC 0
Z9 0
U1 1
U2 5
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0022-460X
EI 1095-8568
J9 J SOUND VIB
JI J. Sound Vibr.
PD SEP 29
PY 2015
VL 353
BP 243
EP 258
DI 10.1016/j.jsv.2015.05.011
PG 16
WC Acoustics; Engineering, Mechanical; Mechanics
SC Acoustics; Engineering; Mechanics
GA CM5QQ
UT WOS:000357743900014
ER
PT J
AU Christou, AA
Killen, RM
Burger, MH
AF Christou, Apostolos A.
Killen, Rosemary M.
Burger, Matthew H.
TI The meteoroid stream of comet Encke at Mercury: Implications for MErcury
Surface, Space ENvironment, GEochemistry, and Ranging observations of
the exosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE comets; dynamics; Mercury; atmospheres
ID CALCIUM EXOSPHERE; TAURID COMPLEX; INTERPLANETARY DUST; BROKEN COMETS;
SOLAR-SYSTEM; SHOWERS; EVOLUTION; ORIGIN; POLARIMETRY; ATMOSPHERE
AB We test the hypothesis that an annually repeatable Ca emission excess in Mercury's exosphere at a True Anomaly Angle (TAA) of 25 degrees 5 degrees is due to particles from comet 2P/Encke impacting the surface. By simulating the dynamical evolution of Encke particles under planetary perturbations and Poynting-Robertson drag, we find that millimeter-sized grains ejected 1-2x10(4)years ago encounter Mercury at TAA=350 degrees-30 degrees. The timing of the excess emission is consistent with a major dust release episode less than or similar to 20kyr ago, possibly due to Encke progenitor breakup. The emission mechanism is likely the direct injection of impact-liberated Ca into sunlight rather than nightside surface adsorption for subsequent release at dawn. The timing of dust release from the comet depends on this mechanism; a 10kyr age is implied by the direct-injection scenario.
C1 [Christou, Apostolos A.] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Killen, Rosemary M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Burger, Matthew H.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA.
RP Christou, AA (reprint author), Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland.
EM aac@arm.ac.uk
FU Northern Ireland Department of Culture, Arts and Leisure (DCAL); NASA
[NNX07AR78G-S01]; SFI/HEA Irish Centre for High-End Computing (ICHEC);
Dublin Institute for Advanced Studies (DIAS)
FX We thank the two reviewers for their comments which improved the paper
and David Asher for discussions on the age of the Encke stream.
Astronomical research at the Armagh Observatory is funded by the
Northern Ireland Department of Culture, Arts and Leisure (DCAL). R.M.K.
was supported by NASA grant NNX07AR78G-S01 as a Participating Scientist
on the NASA MESSENGER mission to Mercury and by STROFIO, a NASA Mission
of Opportunity on the BepiColombo mission. A.A.C. acknowledges the
SFI/HEA Irish Centre for High-End Computing (ICHEC) as well as the
Dublin Institute for Advanced Studies (DIAS) for the provision of
computational facilities and support.
NR 49
TC 3
Z9 3
U1 2
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 28
PY 2015
VL 42
IS 18
BP 7311
EP 7318
DI 10.1002/2015GL065361
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GN
UT WOS:000363412400010
ER
PT J
AU Daerden, F
Whiteway, JA
Neary, L
Komguem, L
Lemmon, MT
Heavens, NG
Cantor, BA
Hebrard, E
Smith, MD
AF Daerden, F.
Whiteway, J. A.
Neary, L.
Komguem, L.
Lemmon, M. T.
Heavens, N. G.
Cantor, B. A.
Hebrard, E.
Smith, M. D.
TI A solar escalator on Mars: Self-lifting of dust layers by radiative
heating
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Mars; lidar; dust layers; solar escalator; radiative heating
ID GENERAL-CIRCULATION MODEL; MARTIAN ATMOSPHERE; GEM MODEL; ICE; CYCLE
AB Dust layers detected in the atmosphere of Mars by the light detection and ranging (LIDAR) instrument on the Phoenix Mars mission are explained using an atmospheric general circulation model. The layers were traced back to observed dust storm activity near the edge of the north polar ice cap where simulated surface winds exceeded the threshold for dust lifting by saltation. Heating of the atmospheric dust by solar radiation caused buoyant instability and mixing across the top of the planetary boundary layer (PBL). Differential advection by wind shear created detached dust layers above the PBL that ascended due to radiative heating and arrived at the Phoenix site at heights corresponding to the LIDAR observations. The self-lifting of the dust layers is similar to the solar escalator mechanism for aerosol layers in the Earth's stratosphere.
C1 [Daerden, F.; Neary, L.] Belgian Inst Space Aeron, Brussels, Belgium.
[Whiteway, J. A.; Komguem, L.] York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 2R7, Canada.
[Lemmon, M. T.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX USA.
[Heavens, N. G.] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA.
[Cantor, B. A.] Malin Space Sci Syst, San Diego, CA USA.
[Hebrard, E.; Smith, M. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hebrard, E.] Oak Ridge Associated Univ, NASA Postdoctoral Program, Oak Ridge, TN USA.
RP Daerden, F (reprint author), Belgian Inst Space Aeron, Brussels, Belgium.
EM Frank.Daerden@aeronomie.be
RI Lemmon, Mark/E-9983-2010; HEBRARD, Eric/E-9257-2014;
OI Lemmon, Mark/0000-0002-4504-5136; HEBRARD, Eric/0000-0003-0770-7271;
Heavens, Nicholas/0000-0001-7654-503X
FU Belgian Federal Science Policy Office (BELSPO) [MO/35/029]; Space
Science Enhancement Program of the Canadian Space Agency (CSA); CSA
[9F007-070437/001/SR]
FX The model output used in this paper is available by request from author
Daerden. The LIDAR, SSI, and MCS data used in this paper are freely
available on the NASA Planetary Data System. The MARCI images used in
this paper are available by request from author Cantor. This research
was carried out with support from the Belgian Federal Science Policy
Office (BELSPO) under grant MO/35/029 and from the Space Science
Enhancement Program of the Canadian Space Agency (CSA). Support for the
LIDAR instrument Science Team during the Phoenix mission was provided by
the CSA under contract 9F007-070437/001/SR. The Phoenix mission was led
by Peter H. Smith at the University of Arizona, on behalf of NASA, and
managed by the Jet Propulsion Laboratory.
NR 50
TC 6
Z9 6
U1 5
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 28
PY 2015
VL 42
IS 18
BP 7319
EP 7326
DI 10.1002/2015GL064892
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GN
UT WOS:000363412400011
ER
PT J
AU Morgan, GA
Campbell, BA
Carter, LM
Plaut, JJ
AF Morgan, Gareth A.
Campbell, Bruce A.
Carter, Lynn M.
Plaut, Jeffrey J.
TI Evidence for the episodic erosion of the Medusae Fossae Formation
preserved within the youngest volcanic province on Mars
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Mars surface; Mars volcanism; Medusae Fossae Formation; orbital radar
sounder
ID CERBERUS FOSSAE; SHALLOW RADAR; DEPOSITS; LAVA; GROUNDWATER;
EMPLACEMENT; HISTORY; SHARAD; WATER; SEA
AB We use orbital SHAllow RADar (SHARAD) sounder data to three-dimensionally visualize the subsurface structure of Elysium Planitia, the youngest volcanic province on Mars. Our results reveal an emplacement history consisting of multiple groups of overlapping lava flow units, originating from different sources. The uniquely complex radar stratigraphy of Elysium Planitia, relative to other volcanic regions, requires a distinct mechanism to generate the numerous reflectors observed in SHARAD data. Sedimentary deposits interbedded with successive batches of lava flows could account for the elaborate pattern of reflectors. We infer that widespread, rapidly emplaced material sourced from the enigmatic Medusae Fossae Formation (MFF) creates these sedimentary layers. This implies that episodes of atmospheric activity, perhaps linked with the obliquity of Mars, periodically erode and redeposit material from the MFF across a large region.
C1 [Morgan, Gareth A.; Campbell, Bruce A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Plaut, Jeffrey J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Morgan, GA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
EM morganga@si.edu
RI Carter, Lynn/D-2937-2012
FU NASA's Mars Data Analysis program
FX We wish to thank the four reviewers for their very helpful comments and
suggestions. All the data used in this study are available through
NASA's Planetary Data System. We gratefully acknowledge financial
support provided by a grant from NASA's Mars Data Analysis program. The
MFF map element incorporated within Figure 1 was reprinted from Vaucher,
J., D. Baratoux, N. Mangold, P. Pinet, K. Kurita, and M. Gregoire, The
volcanic history of central Elysium Planitia: Implications for Martian
magmatism, Icarus, 204, 418-442 (2009) with permission from Elsevier.
NR 27
TC 2
Z9 2
U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 28
PY 2015
VL 42
IS 18
BP 7336
EP 7342
DI 10.1002/2015GL065017
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GN
UT WOS:000363412400013
ER
PT J
AU Maeda, EE
Kim, H
Aragao, LEOC
Famiglietti, JS
Oki, T
AF Maeda, Eduardo Eiji
Kim, Hyungjun
Aragao, Luiz E. O. C.
Famiglietti, James S.
Oki, Taikan
TI Disruption of hydroecological equilibrium in southwest Amazon mediated
by drought
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE GRACE; QSCAT; drought; water deficit; Amazon
ID RAIN-FOREST; TROPICAL FORESTS; BASIN; EVAPOTRANSPIRATION; SEASONALITY;
VARIABILITY; SENSITIVITY; MORTALITY; CANOPY
AB The impacts of droughts on the Amazon ecosystem have been broadly discussed in recent years, but a comprehensive understanding of the consequences is still missing. In this study, we show evidence of a fragile hydrological equilibrium in the western Amazon. While drainage systems located near the equator and the western Amazon do not show water deficit in years with average climate conditions, this equilibrium can be broken during drought events. More importantly, we show that this effect is persistent, taking years until the normal hydrological patterns are reestablished. We show clear links between persistent changes in forest canopy structure and changes in hydrological patterns, revealing physical evidence of hydrological mechanisms that may lead to permanent changes in parts of the Amazon ecosystem. If prospects of increasing drought frequency are confirmed, a change in the current hydroecological patterns in the western Amazon could take place in less than a decade.
C1 [Maeda, Eduardo Eiji] Univ Helsinki, Dept Geosci & Geog, Helsinki, Finland.
[Kim, Hyungjun; Oki, Taikan] Univ Tokyo, Inst Ind Sci, Tokyo, Japan.
[Aragao, Luiz E. O. C.] Natl Inst Space Res INPE, Sao Jose Dos Campos, Brazil.
[Aragao, Luiz E. O. C.] Univ Exeter, Coll Life & Environm Sci, Exeter, Devon, England.
[Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Famiglietti, James S.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA.
RP Maeda, EE (reprint author), Univ Helsinki, Dept Geosci & Geog, Helsinki, Finland.
EM eduardo.maeda@helsinki.fi
RI Oki, Taikan/E-5778-2010; Maeda, Eduardo/E-7327-2011
OI Oki, Taikan/0000-0003-4067-4678; Maeda, Eduardo/0000-0001-7932-1824
FU Academy of Finland; UK NERC [NE/l018123/1]; CNPq; FAPESP [2013/50533-5];
Japan Society for the Promotion of Science [23226012]; Ministry of
Education, Culture, Sports, Science and Technology SOUSEI Program
FX This study was financially supported by the Academy of Finland.
L.E.O.C.A. acknowledges the support of the UK NERC (grant NE/l018123/1)
and the CNPq Fellowship and FAPESP (grant 2013/50533-5). H.K. and T.O.
were jointly supported by Japan Society for the Promotion of Science
KAKENHI (23226012) and Ministry of Education, Culture, Sports, Science
and Technology SOUSEI Program. GRACE land data were processed by Sean
Swenson, supported by the NASA MEaSUREs Program, and are available at
http://grace.jpl.nasa.gov. The authors are thankful for the insightful
comments and suggestions of the anonymous reviewers.
NR 36
TC 3
Z9 3
U1 4
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 28
PY 2015
VL 42
IS 18
BP 7546
EP 7553
DI 10.1002/2015GL065252
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GN
UT WOS:000363412400039
ER
PT J
AU Kwok, R
AF Kwok, Ron
TI Sea ice convergence along the Arctic coasts of Greenland and the
Canadian Arctic Archipelago: Variability and extremes (1992-2014)
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Arctic sea ice; ice convergence; ice thickness distribution; melt ponds
ID OCEAN; RETRIEVALS; THICKNESS
AB After the summer of 2013, a convergence-induced tail in the thickness distribution of the ice cover is found along the Arctic coasts of Greenland and Canadian Arctic Archipelago. Prompted by this, a normalized ice convergence index (ICI) is introduced to examine the variability and extremes in convergence in a 23year record (1992-2014) of monthly ice drift. Large-scale composites of circulation patterns, characteristic of regional convergence and divergence, are examined. Indeed, the ICI shows the June 2013 convergence event to be an extreme (i.e., ICI>2). Furthermore, there is a cluster of 9months over a 17month period with positive ICIs (i.e., >1) following the record summer minimum ice extent (SMIE) in 2012; the imprint of ice dynamics from this cluster of positive ICIs likely contributed to higher SMIEs in 2013 and 2014. The impact of convergence on SMIE is discussed, and the increase in Arctic ice volume in 2013 is underscored.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM ron.kwok@jpl.nasa.gov
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
NR 20
TC 8
Z9 8
U1 3
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 SEP 28
PY 2015
VL 42
IS 18
BP 7598
EP 7605
DI 10.1002/2015GL065462
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GN
UT WOS:000363412400045
ER
PT J
AU Horton, RM
Coffel, ED
Winter, JM
Bader, DA
AF Horton, Radley M.
Coffel, Ethan D.
Winter, Jonathan M.
Bader, Daniel A.
TI Projected changes in extreme temperature events based on the NARCCAP
model suite
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE climate change and variability; impacts of global change; regional
modeling; climate dynamics
ID NORTHEAST UNITED-STATES; CLIMATE-CHANGE; IMPACT; PRECIPITATION;
VARIABILITY; COLD; ICE
AB Once-per-year (annual) maximum temperature extremes in North American Regional Climate Change Assessment Program (NARCCAP) models are projected to increase more (less) than mean daily maximum summer temperatures over much of the eastern (western) United States. In contrast, the models almost everywhere project greater warming of once-per-year minimum temperatures as compared to mean daily minimum winter temperatures. Under projected changes associated with extremes of the temperature distribution, Baltimore's maximum temperature that was met or exceeded once per year historically is projected to occur 17 times per season by midcentury, a 28% increase relative to projections based on summer mean daily maximum temperature change. Under the same approach, historical once-per-year cold events in Baltimore are projected to occur once per decade. The models are generally able to capture observed geopotential height anomalies associated with temperature extremes in two subregions. Projected changes in extreme temperature events cannot be explained by geopotential height anomalies or lower boundary conditions as reflected by soil moisture anomalies or snow water equivalent.
C1 [Horton, Radley M.; Bader, Daniel A.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10017 USA.
[Horton, Radley M.; Coffel, Ethan D.; Bader, Daniel A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Coffel, Ethan D.] Columbia Univ, Dept Earth & Environm Sci, New York, NY USA.
[Winter, Jonathan M.] Dartmouth Coll, Dept Geog, Hanover, NH 03755 USA.
[Winter, Jonathan M.] Dartmouth Coll, Dept Earth Sci, Hanover, NH 03755 USA.
RP Horton, RM (reprint author), Columbia Univ, Ctr Climate Syst Res, New York, NY 10017 USA.
EM rh142@columbia.edu
FU Department of the Interior Northeast Climate Science Center; NOAA-RISA
Program through the Consortium for Climate Risk in the Urban Northeast
FX This work was supported by the Department of the Interior Northeast
Climate Science Center and the NOAA-RISA Program through the Consortium
for Climate Risk in the Urban Northeast. We acknowledge the regional
climate modeling groups, North American Regional Climate Change
Assessment Program [Mearns and Gutowski, 2009]. We also acknowledge the
global climate modeling groups, the Program for Climate Model Diagnosis,
and Intercomparison (PCMDI) and the WCRP for the CMIP3 multimodel data
set, supported by the Office of Science, U.S. Department of Energy.
NR 52
TC 2
Z9 2
U1 3
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 28
PY 2015
VL 42
IS 18
BP 7722
EP 7731
DI 10.1002/2015GL064914
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GN
UT WOS:000363412400060
ER
PT J
AU Manney, GL
Lawrence, ZD
Santee, ML
Read, WG
Livesey, NJ
Lambert, A
Froidevaux, L
Pumphrey, HC
Schwartz, MJ
AF Manney, Gloria L.
Lawrence, Zachary D.
Santee, Michelle L.
Read, William G.
Livesey, Nathaniel J.
Lambert, Alyn
Froidevaux, Lucien
Pumphrey, Hugh C.
Schwartz, Michael J.
TI A minor sudden stratospheric warming with a major impact: Transport and
polar processing in the 2014/2015 Arctic winter
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE stratospheric sudden warming; Arctic ozone; satellite data
ID OZONE DEPLETION; SATELLITE-OBSERVATIONS; MLS OBSERVATIONS; VORTEX;
MODEL; CLIMATE; SURFACE; MERRA; AREA
AB Stratospheric transport and polar processing during the 2014/2015 Arctic winter were strongly influenced by a minor sudden stratospheric warming (SSW) in early January. Disturbances to temperatures and trace gases in the middle and upper stratosphere were similar in character to those associated with major SSWs: The stratopause dropped, and vertical temperature gradients weakened, followed by renewed descent of mesospheric air. The lower stratospheric polar vortex was barely disrupted and remained unusually strong throughout the winter. The SSW did, however, cause lower stratospheric temperatures to rise well above chlorine activation thresholds; trace gas abundances from the Aura Microwave Limb Sounder (MLS) were consequently exceptional. The degree of chlorine activation in January was the smallest, and lower stratospheric ozone values in February were the highest, in the 11year MLS record. The major role played by a minor SSW highlights the Arctic stratosphere's sensitivity to a spectrum of dynamical variability.
C1 [Manney, Gloria L.] NorthWest Res Associates, Socorro, NM 87011 USA.
[Manney, Gloria L.; Lawrence, Zachary D.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
[Santee, Michelle L.; Read, William G.; Livesey, Nathaniel J.; Lambert, Alyn; Froidevaux, Lucien; Schwartz, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Pumphrey, Hugh C.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland.
RP Manney, GL (reprint author), NorthWest Res Associates, Socorro, NM 87011 USA.
EM manney@nwra.com
RI Schwartz, Michael/F-5172-2016
OI Schwartz, Michael/0000-0001-6169-5094
NR 42
TC 4
Z9 4
U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 28
PY 2015
VL 42
IS 18
BP 7808
EP 7816
DI 10.1002/2015GL065864
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GN
UT WOS:000363412400070
ER
PT J
AU Boulet, C
Ma, Q
Tipping, RH
AF Boulet, C.
Ma, Q.
Tipping, R. H.
TI Line mixing in parallel and perpendicular bands of CO2: A further test
of the refined Robert-Bonamy formalism
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID 20 MU-M; WING REGIONS; SEMICLASSICAL CALCULATIONS; ROTATIONAL
RELAXATION; INFRARED-SPECTRA; SHAPE; PARAMETERS; SYMMETRY; QUANTUM; HE
AB Starting from the refined Robert-Bonamy formalism [Q. Ma, C. Boulet, and R. H. Tipping, J. Chem. Phys. 139, 034305 (2013)], we propose here an extension of line mixing studies to infrared absorptions of linear polyatomic molecules having stretching and bending modes. The present formalism does not neglect the internal degrees of freedom of the perturbing molecules, contrary to the energy corrected sudden (ECS) modelling, and enables one to calculate the whole relaxation matrix starting from the potential energy surface. Meanwhile, similar to the ECS modelling, the present formalism properly accounts for roles played by all the internal angular momenta in the coupling process, including the vibrational angular momentum. The formalism has been applied to the important case of CO2 broadened by N-2. Applications to two kinds of vibrational bands (Sigma -> Sigma and Sigma -> Pi) have shown that the present results are in good agreement with both experimental data and results derived from the ECS model. (C) 2015 AIP Publishing LLC.
C1 [Boulet, C.] CNRS, UMR8214, ISMO, F-91405 Orsay, France.
[Boulet, C.] Univ Paris 11, F-91405 Orsay, France.
[Ma, Q.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Ma, Q.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[Tipping, R. H.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
RP Boulet, C (reprint author), CNRS, UMR8214, ISMO, Bat 350,Campus Orsay, F-91405 Orsay, France.
FU NSF [1228861]; Office of Science of the U.S. Department of Energy
[DE-AC02-05CH11231]
FX Two of the authors (Q. Ma and R. H. Tipping) acknowledge financial
support from NSF under Grant No. 1228861. 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.
NR 36
TC 0
Z9 0
U1 1
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-9606
EI 1089-7690
J9 J CHEM PHYS
JI J. Chem. Phys.
PD SEP 28
PY 2015
VL 143
IS 12
AR 124313
DI 10.1063/1.4931587
PG 12
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA CT1OL
UT WOS:000362568100030
PM 26429017
ER
PT J
AU Jin, J
Saglamyurek, E
Puigibert, ML
Verma, V
Marsili, F
Nam, SW
Oblak, D
Tittel, W
AF Jin, Jeongwan
Saglamyurek, Erhan
Puigibert, Marcel. li Grimau
Verma, Varun
Marsili, Francesco
Nam, Sae Woo
Oblak, Daniel
Tittel, Wolfgang
TI Telecom-Wavelength Atomic Quantum Memory in Optical Fiber for Heralded
Polarization Qubits
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID PHOTONS; TELEPORTATION; EFFICIENCY
AB Polarization-encoded photons at telecommunication wavelengths provide a compelling platform for practical realizations of photonic quantum information technologies due to the ease of performing single qubit manipulations, the availability of polarization-entangled photon-pair sources, and the possibility of leveraging existing fiber-optic links for distributing qubits over long distances. An optical quantum memory compatible with this platform could serve as a building block for these technologies. Here we present the first experimental demonstration of an atomic quantum memory that directly allows for reversible mapping of quantum states encoded in the polarization degree of freedom of a telecom-wavelength photon. We show that heralded polarization qubits at a telecom wavelength are stored and retrieved with near-unity fidelity by implementing the atomic frequency comb protocol in an ensemble of erbium atoms doped into an optical fiber. Despite remaining limitations in our proof-of-principle demonstration such as small storage efficiency and storage time, our broadband light-matter interface reveals the potential for use in future quantum information processing.
C1 [Jin, Jeongwan; Saglamyurek, Erhan; Puigibert, Marcel. li Grimau; Oblak, Daniel; Tittel, Wolfgang] Univ Calgary, Inst Quantum Sci & Technol, Calgary, AB T2N 1N4, Canada.
[Jin, Jeongwan; Saglamyurek, Erhan; Puigibert, Marcel. li Grimau; Oblak, Daniel; Tittel, Wolfgang] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Verma, Varun; Nam, Sae Woo] Natl Inst Stand & Technol, Boulder, CO 80305 USA.
[Marsili, Francesco] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jin, J (reprint author), Univ Waterloo, Dept Phys & Astron, Inst Quantum Comp, 200 Univ Ave West, Waterloo, ON, Canada.
EM wtittel@ucalgary.ca
RI Tittel, Wolfgang/A-1600-2011
FU Alberta Innovates Technology Futures (AITF); National Science and
Engineering Research Council of Canada (NSERC); Canadian Institute for
Advanced Research (CIFAR); Defense Advanced Research Projects Agency
(DARPA)
FX We thank Raju Valivarthi, Qiang Zhou, Matthew D. Shaw, and Vladimir
Kiselyov for useful discussions and technical support, and gratefully
acknowledge support through Alberta Innovates Technology Futures (AITF)
and the National Science and Engineering Research Council of Canada
(NSERC). W. T. acknowledges support as a Canadian Institute for Advanced
Research (CIFAR) senior fellow. V. B. V. and S. W. N. acknowledge
partial funding for detector development from the Defense Advanced
Research Projects Agency (DARPA) Information in a Photon (InPho)
program. Part of the research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 28
TC 8
Z9 8
U1 6
U2 20
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD SEP 28
PY 2015
VL 115
IS 14
AR 140501
DI 10.1103/PhysRevLett.115.140501
PG 5
WC Physics, Multidisciplinary
SC Physics
GA CS1HT
UT WOS:000361815100001
PM 26551798
ER
PT J
AU Ganeshan, M
Wu, DL
AF Ganeshan, Manisha
Wu, Dong L.
TI An investigation of the Arctic inversion using COSMIC RO observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Arctic; inversion; COSMIC RO; surface-based inversion; refractivity; GPS
ID ATMOSPHERIC BOUNDARY-LAYER; TEMPERATURE INVERSIONS; ANNUAL CYCLE;
SEA-ICE; CLOUD; OCEAN; STRENGTH; VARIABILITY; SENSITIVITY
AB The stable temperature inversion over sea ice plays an important role in the surface climate of the Arctic Ocean through direct and indirect feedbacks. Although several studies have investigated Arctic inversion characteristics such as height, depth, and frequency, there are significant challenges for long-term climate monitoring mainly due to limited sampling over the ocean and/or poor resolution of available observations. This study investigates the Arctic temperature inversion during the cold season using the high-resolution refractivity profiles from Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC) radio occultation (RO). For the coldest and driest months in the Arctic, a reliable retrieval technique for boundary layer properties, such as inversion height and surface-based inversion (SBI) frequency, is developed. We find that these variables have a strong negative relationship over the Arctic Ocean and are well correlated in the time and space domain. The spatial patterns show a minimum inversion height (maximum SBI frequency) over the ice-covered Pacific sector of the ocean similar to that observed in past studies. Seasonal evolution of the inversion characteristics suggests a surface temperature control over the sea ice region, with the peak in SBI frequency occurring during the transition period from winter to spring. There is little diurnal variability in the mean inversion height during the cold season. Despite its limitations, the RO refractivity profile is found quite useful for monitoring the Arctic boundary layer, including interannual variability of inversion characteristics.
C1 [Ganeshan, Manisha] USRA, Goddard Earth Sci Technol & Res Studies & Invest, Greenbelt, MD 20771 USA.
[Wu, Dong L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ganeshan, M (reprint author), USRA, Goddard Earth Sci Technol & Res Studies & Invest, Greenbelt, MD 20771 USA.
EM mganeshan@usra.edu
RI Wu, Dong/D-5375-2012
FU NASA's GNSS Remote Sensing and Interdisciplinary Research in Earth
Science programs
FX This work is supported by NASA's GNSS Remote Sensing and
Interdisciplinary Research in Earth Science programs. COSMIC RO data
used in this study were acquired from University Corporation for
Atmospheric Research (http://www.cosmic.ucar.edu/). SHEBA data were
obtained from NOAA's National Climatic Data Center
(http://www.esrl.noaa.gov/psd/arctic/sheba/).
NR 31
TC 1
Z9 1
U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 27
PY 2015
VL 120
IS 18
BP 9338
EP 9351
DI 10.1002/2015JD023058
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU3LE
UT WOS:000363425900018
ER
PT J
AU Liu, CL
Allan, RP
Berrisford, P
Mayer, M
Hyder, P
Loeb, N
Smith, D
Vidale, PL
Edwards, JM
AF Liu, Chunlei
Allan, Richard P.
Berrisford, Paul
Mayer, Michael
Hyder, Patrick
Loeb, Norman
Smith, Doug
Vidale, Pier-Luigi
Edwards, John M.
TI Combining satellite observations and reanalysis energy transports to
estimate global net surface energy fluxes 1985-2012
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE surface heat flux; satellite observations; climate models; energy
imbalance
ID PACIFIC COLD-TONGUE; OCEAN HEAT-CONTENT; MODEL DESCRIPTION; WARMING
HIATUS; CLIMATE MODEL; DECADAL VARIABILITY; COUPLED MODEL; SYSTEM MODEL;
ERA-INTERIM; PAST DECADE
AB Two methods are developed to estimate net surface energy fluxes based upon satellite-derived reconstructions of radiative fluxes at the top of atmosphere and the atmospheric energy tendencies and transports from the ERA-Interim reanalysis. Method 1 applies the mass-adjusted energy divergence from ERA-Interim, while method 2 estimates energy divergence based upon the net energy difference at the top of atmosphere and the surface from ERA-Interim. To optimize the surface flux and its variability over ocean, the divergences over land are constrained to match the monthly area mean surface net energy flux variability derived from a simple relationship between the surface net energy flux and the surface temperature change. The energy divergences over the oceans are then adjusted to remove an unphysical residual global mean atmospheric energy divergence. The estimated net surface energy fluxes are compared with other data sets from reanalysis and atmospheric model simulations. The spatial correlation coefficients of multiannual means between the estimations made here and other data sets are all around 0.9. There are good agreements in area mean anomaly variability over the global ocean, but discrepancies in the trend over the eastern Pacific are apparent.
C1 [Liu, Chunlei; Allan, Richard P.; Vidale, Pier-Luigi] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Allan, Richard P.] Nat Ctr Earth Observat, Reading, Berks, England.
[Allan, Richard P.; Berrisford, Paul; Vidale, Pier-Luigi] Natl Ctr Atmospher Sci, Reading, Berks, England.
[Berrisford, Paul] ECMWF, Reading, Berks, England.
[Mayer, Michael] Univ Vienna, Dept Meteorol & Geophys, Vienna, Austria.
[Hyder, Patrick; Smith, Doug; Edwards, John M.] Met Off, Exeter, Devon, England.
[Loeb, Norman] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Liu, CL (reprint author), Univ Reading, Dept Meteorol, Reading, Berks, England.
EM c.l.liu@reading.ac.uk
RI Allan, Richard/B-5782-2008;
OI Allan, Richard/0000-0003-0264-9447; Vidale, Pier
Luigi/0000-0002-1800-8460
FU Natural Environment Research Council DEEP-C grant [NE/K005480/1];
National Centre for Earth Observation; National Centre for Atmospheric
Science; joint DECC/Defra Met Office Hadley Centre Climate Programme
[GA01101]
FX This work was supported by the Natural Environment Research Council
DEEP-C grant NE/K005480/1, the National Centre for Earth Observation,
and the National Centre for Atmospheric Science. D.S. and P.H. were
supported by the joint DECC/Defra Met Office Hadley Centre Climate
Programme (GA01101). Special thanks to our colleague Kevin Hodges for
supplying the Hoskins spectral filter code. We acknowledge the World
Climate Research Programme's Working Group on AMIP5 data, and we thank
the climate modeling groups (models listed in Table 1) for producing and
making available their model outputs. The UPSCALE simulations were
performed under a grant of supercomputing time from PRACE using the HLRS
HERMIT Cray XE6. We acknowledge the ECMWF for providing ERA-Interim and
ERA20C data and NASA scientists for MERRA data. We thank Valerio
Lucarini and another anonymous reviewer for reviewing this paper and
providing constructive comments and suggestions. Data generated by this
work are available at http://www.met.reading.ac.uk/similar to
sgs02rpa/research/DEEP-C/GRL/.
NR 80
TC 7
Z9 7
U1 3
U2 23
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 27
PY 2015
VL 120
IS 18
BP 9374
EP 9389
DI 10.1002/2015JD023264
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU3LE
UT WOS:000363425900020
ER
PT J
AU Wang, Y
Jiang, JH
Su, H
AF Wang, Yuan
Jiang, Jonathan H.
Su, Hui
TI Atmospheric responses to the redistribution of anthropogenic aerosols
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE anthropogenic aerosols; general circulation model; radiative forcing;
aerosol-cloud interaction
ID ASIAN SUMMER MONSOON; CLIMATE SIMULATIONS; GLOBAL CLIMATE; CMIP5 MODELS;
PARAMETERIZATION; PRECIPITATION; CIRCULATION; EMISSIONS; REPRESENTATION;
MICROPHYSICS
AB The geographical shift of global anthropogenic aerosols from the developed countries to the Asian continent since the 1980s could potentially perturb the regional and global climate due to aerosol-cloud-radiation interactions. We use an atmospheric general circulation model with different aerosol scenarios to investigate the radiative and microphysical effects of anthropogenic aerosols from different regions on the radiation budget, precipitation, and large-scale circulations. An experiment contrasting anthropogenic aerosol scenarios in 1970 and 2010 shows that the altered cloud reflectivity and solar extinction by aerosols results in regional surface temperature cooling in East and South Asia, and warming in the US and Europe, respectively. These aerosol-induced temperature changes are consistent with the relative temperature trends from 1980 to 2010 over different regions in the reanalysis data. A reduced meridional streamfunction and zonal winds over the tropics as well as a poleward shift of the jet stream suggest weakened and expanded tropical circulations, which are induced by the redistributed aerosols through a relaxing of the meridional temperature gradient. Consequently, precipitation is suppressed in the deep tropics and enhanced in the subtropics. Our assessments of the aerosol effects over the different regions suggest that the increasing Asian pollution accounts for the weakening of the tropics circulation, while the decreasing pollution in Europe and US tends to shift the circulation systems southward. Moreover, the aerosol indirect forcing is predominant over the total aerosol forcing in magnitude, while aerosol radiative and microphysical effects jointly shape the meridional energy distributions and modulate the circulation systems.
C1 [Wang, Yuan; Jiang, Jonathan H.; Su, Hui] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wang, Y (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM yuan.wang@jpl.nasa.gov
FU NASA ROSES14-ACMAP
FX We appreciate the funding support by the NASA ROSES14-ACMAP. The
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. The simulations are performed on NASA Pleiades
Supercomputer. We thank Jonathan Murphy from JPL for English editing.
All model results are archived at the JPL cluster and available upon
request. Please contact Yuan Wang at yuan.wang@jpl.nasa.gov to access
the modeling data.
NR 47
TC 4
Z9 4
U1 7
U2 25
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 27
PY 2015
VL 120
IS 18
BP 9625
EP 9641
DI 10.1002/2015JD023665
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU3LE
UT WOS:000363425900034
ER
PT J
AU Schoeberl, MR
Selkirk, HB
Vomel, H
Douglass, AR
AF Schoeberl, Mark R.
Selkirk, Henry B.
Voemel, Holger
Douglass, Anne R.
TI Sources of seasonal variability in tropical upper troposphere and lower
stratosphere water vapor and ozone: Inferences from the Ticosonde data
set at Costa Rica
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE tropical tropopause; water vapor; ozone
ID TROPOPAUSE LAYER; EFFECTIVE DIFFUSIVITY; DEHYDRATION; CLIMATOLOGY;
TRANSPORT; ICE
AB We present an analysis of joint balloonsonde profiles of water vapor and ozone made at Costa Rica from 2005 to 2011 using compositing techniques, tracer-tracer diagrams, and back trajectory methods. Our analysis reveals important seasonal differences in structure in the upper troposphere and lower stratosphere. Water vapor amounts in boreal winter at Costa Rica are much lower than expected from local ice saturation temperatures. The boreal summer data show both higher average water vapor amounts and a much higher level of variability than the winter data. To understand this seasonal contrast, we consider three sources of tracer variability: wave-induced vertical motion across strong vertical gradients (wave variability), differences in source air masses resulting from horizontal transport (source variability), and changes induced along parcel paths due to physical processes (path variability). The winter and summer seasons show different mixes of these three sources of variability with more air originating in the tropical western Pacific during winter.
C1 [Schoeberl, Mark R.] Sci & Technol Corp, Columbia, MD 21046 USA.
[Selkirk, Henry B.] GESTAR NASA GSFC, Greenbelt, MD USA.
[Voemel, Holger] NCAR Earth Observat Lab, Boulder, CO USA.
[Douglass, Anne R.] NASA GSFC, Greenbelt, MD USA.
RP Schoeberl, MR (reprint author), Sci & Technol Corp, Columbia, MD 21046 USA.
EM mark.schoeberl@mac.com
RI Douglass, Anne/D-4655-2012
FU Instituto Meteorologico Nacional, Universidad de Costa Rica; Universidad
Nacional; NASA; Comite Regional de Recursos Hidraulicos
FX The authors would like to acknowledge the dedicated efforts of the
extended group who worked together to create the Ticosonde data set.
This has included, among many others, Jessica Valverde, Werner Stolz,
Jorge Andres Diaz, and Gary Morris; Walter Fernandez, Jorge Amador, and
Eladio Zarate; Leonhard Pfister, Randy May, Grace S. Peng, Jimena Lopez,
and Marion Legg; Victor Hugo Beita, Karla Cerna, Diana Gonzales, Jose
Pablo Sibaja, Ilena Vega, Rosa Alfaro, and Sebastian Miranda; Juan
Valdes, Victor Hernandez, Kristel Heinrich, Marcial Garbanzo and Gustavo
Garbanzo; and Ernesto Corrales, Yetty Madrigal, and Sara Azofeifa. We
also acknowledge support from the following institutions in Costa Rica:
Instituto Meteorologico Nacional, Universidad de Costa Rica, Universidad
Nacional, and Comite Regional de Recursos Hidraulicos. M.R.S. would also
like to acknowledge the use of the Texas A&M computers to perform the
trajectory calculations. Finally, H.B.S. would like to thank Karen
Rosenlof of the NOAA Earth Sciences Research Laboratory for the use of
her lapse rate tropopause code. We would also like to thank the
anonymous reviewers for their many helpful comments. This work was
supported by NASA's Upper Atmosphere Research Program and the Radiation
Sciences Program. The MLS data are available through
http://mls.jpl.nasa.gov. Ticosonde sounding data are available through
the Aura Validation Data Center (AVDC, http://avdc.gsfc.nasa.gov) at
NASA Goddard Space Flight Center.
NR 49
TC 1
Z9 1
U1 2
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 SEP 27
PY 2015
VL 120
IS 18
BP 9684
EP 9701
DI 10.1002/2015JD023299
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU3LE
UT WOS:000363425900038
ER
PT J
AU Miller, DJ
Sun, K
Tao, L
Pan, D
Zondlo, MA
Nowak, JB
Liu, Z
Diskin, G
Sachse, G
Beyersdorf, A
Ferrare, R
Scarino, AJ
AF Miller, David J.
Sun, Kang
Tao, Lei
Pan, Da
Zondlo, Mark A.
Nowak, John B.
Liu, Zhen
Diskin, Glenn
Sachse, Glen
Beyersdorf, Andreas
Ferrare, Richard
Scarino, Amy Jo
TI Ammonia and methane dairy emission plumes in the San Joaquin Valley of
California from individual feedlot to regional scales
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE emission plumes; dairy; feedlot; methane; ammonia; emission ratios
ID COVARIANCE FLUX MEASUREMENTS; GREENHOUSE-GAS EMISSIONS; QUANTUM
CASCADE-LASER; OPEN-PATH; ATMOSPHERIC AMMONIA; SATELLITE-OBSERVATIONS;
PRODUCTION FACILITY; SOUTHERN IDAHO; UNITED-STATES; MOBILE
AB Agricultural ammonia (NH3) emissions are highly uncertain, with high spatiotemporal variability and a lack of widespread in situ measurements. Regional NH3 emission estimates using mass balance or emission ratio approaches are uncertain due to variable NH3 sources and sinks as well as unknown plume correlations with other dairy source tracers. We characterize the spatial distributions of NH3 and methane (CH4) dairy plumes using in situ surface and airborne measurements in the Tulare dairy feedlot region of the San Joaquin Valley, California, during the NASA Deriving Information on Surface conditions from Column and Vertically Resolved Observations Relevant to Air Quality 2013 field campaign. Surface NH3 and CH4 mixing ratios exhibit large variability with maxima localized downwind of individual dairy feedlots. The geometric mean NH3:CH4 enhancement ratio derived from surface measurements is 0.15 0.03ppmvppmv(-1). Individual dairy feedlots with spatially distinct NH3 and CH4 source pathways led to statistically significant correlations between NH3 and CH4 in 68% of the 69 downwind plumes sampled. At longer sampling distances, the NH3:CH4 enhancement ratio decreases 20-30%, suggesting the potential for NH3 deposition as a loss term for plumes within a few kilometers downwind of feedlots. Aircraft boundary layer transect measurements directly above surface mobile measurements in the dairy region show comparable gradients and geometric mean enhancement ratios within measurement uncertainties, even when including NH3 partitioning to submicron particles. Individual NH3 and CH4 plumes sampled at close proximity where losses are minimal are not necessarily correlated due to lack of mixing and distinct source pathways. Our analyses have important implications for constraining NH3 sink and plume variability influences on regional NH3 emission estimates and for improving NH3 emission inventory spatial allocations.
C1 [Miller, David J.; Sun, Kang; Tao, Lei; Pan, Da; Zondlo, Mark A.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
[Nowak, John B.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO USA.
[Liu, Zhen] Sandia Natl Labs, Combust Res Facil, Livermore, CA USA.
[Diskin, Glenn; Beyersdorf, Andreas; Ferrare, Richard; Scarino, Amy Jo] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Sachse, Glen] Natl Inst Aerosp, Hampton, VA USA.
[Scarino, Amy Jo] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Zondlo, MA (reprint author), Brown Univ, Inst Brown Environm & Soc, Providence, RI 02912 USA.
EM mzondlo@princeton.edu
RI Liu, Zhen/C-3027-2011; Nowak, John/B-1085-2008; Zondlo, Mark/R-6173-2016
OI Nowak, John/0000-0002-5697-9807; Zondlo, Mark/0000-0003-2302-9554
FU NSF Center for Mid-Infrared Technologies for Health and the Environment
(MIRTHE, NSF-ERC) [EEC-0540832]; National Science Foundation
[DGE-0646086]; NASA Earth and Space Science Fellowship [IIP-1263579];
Sandia Laboratory Directed Research and Development (LDRD) Program;
National Nuclear Security Administration [DE-AC04-94-AL85000]; NASA
[NNX14AT36G]
FX We acknowledge the support of James Crawford and the DISCOVER-AQ 2013
science team, as well as Trent Proctor (USFS) for providing space for
field calibrations in Porterville, California. The authors thank Bruce
Anderson for use of the PILS/IC NH4+ data and
Nathan Trevino (San Joaquin Valley Unified Air Pollution Control
District) for use of the ground-based wind observations. All data used
in the analyses are publicly available at
http://www-air.larc.nasa.gov/cgi-bin/ArcView/discover-aq.ca-2013 [NASA
Archive, 2014]. We also thank LICOR Biosciences for use of the LI-7700
methane analyzer and Professor Elie Bou-Zeid for use of the LI-7500
CO2/H2O analyzer. We acknowledge logistical
assistance and helpful discussions with Paul Ginoux, James Kelly, Joshua
DiGangi, Anthony O'Brien, Minghui Diao, James Smith and his research
group, and Claire Gmachl and her research group. This research is
supported by the NSF Center for Mid-Infrared Technologies for Health and
the Environment (MIRTHE, NSF-ERC) under grant EEC-0540832. D.J. Miller
acknowledges support by the National Science Foundation Graduate
Research Fellowship under grant DGE-0646086. K. Sun acknowledges support
by NASA Earth and Space Science Fellowship IIP-1263579. The authors
acknowledge the support of Hope Michelsen and Ray Bambha for the work on
WRF simulations at Sandia National Laboratories that was funded by the
Sandia Laboratory Directed Research and Development (LDRD) Program.
Sandia is a multiprogram laboratory operated by Sandia Corporation, a
Lockheed Martin Company, for the National Nuclear Security
Administration under contract DE-AC04-94-AL85000. D.P. and M.Z.
acknowledge support through NASA NNX14AT36G. Finally, we thank three
anonymous reviewers for very helpful feedback on this manuscript.
NR 76
TC 4
Z9 4
U1 9
U2 29
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 27
PY 2015
VL 120
IS 18
BP 9718
EP 9738
DI 10.1002/2015JD023241
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU3LE
UT WOS:000363425900040
ER
PT J
AU Kemp, KC
Baek, SB
Lee, WG
Meyyappan, M
Kim, KS
AF Kemp, K. Christian
Baek, Seung Bin
Lee, Wang-Geun
Meyyappan, M.
Kim, Kwang S.
TI Activated carbon derived from waste coffee grounds for stable methane
storage
SO NANOTECHNOLOGY
LA English
DT Article
DE adsorption; activated carbon; methane storage; energy storage;
mechanism; hydrogen storage
ID METAL-ORGANIC FRAMEWORK; CHEMICAL ACTIVATION; HYDROGEN STORAGE;
GAS-STORAGE; MICROPOROUS CARBON; NATURAL-GAS; AIR-QUALITY; PORE-SIZE;
ADSORPTION; GRAPHENE
AB An activated carbon material derived from waste coffee grounds is shown to be an effective and stable medium for methane storage. The sample activated at 900 degrees C displays a surface area of 1040.3 m(2) g(-1) and a micropore volume of 0.574 cm(3) g(-1) and exhibits a stable CH4 adsorption capacity of similar to 4.2 mmol g(-1) at 3.0 MPa and a temperature range of 298 +/- 10 K. The same material exhibits an impressive hydrogen storage capacity of 1.75 wt% as well at 77 K and 100 kPa. Here, we also propose a mechanism for the formation of activated carbon from spent coffee grounds. At low temperatures, the material has two distinct types with low and high surface areas; however, activation at elevated temperatures drives off the low surface area carbon, leaving behind the porous high surface area activated carbon.
C1 [Kemp, K. Christian; Baek, Seung Bin; Lee, Wang-Geun; Kim, Kwang S.] UNIST, Sch Nat Sci, Dept Chem, Ulsan 689798, South Korea.
[Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kemp, KC (reprint author), Pohang Univ Sci & Technol POSTECH, Dept Environm Engn, Pohang, South Korea.
EM kimks@unist.ac.kr
RI Kim, Kwang/C-7538-2012
OI Kim, Kwang/0000-0002-6929-5359
FU NRF [2010-0020414]
FX This work was supported by NRF (National Honor Scientist Program:
2010-0020414).
NR 41
TC 1
Z9 1
U1 5
U2 33
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 SEP 25
PY 2015
VL 26
IS 38
AR 385602
DI 10.1088/0957-4484/26/38/385602
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA CR0MN
UT WOS:000361012900014
PM 26329310
ER
PT J
AU Tinto, M
de Araujo, JCN
Kuga, HK
Alves, MES
Aguiar, OD
AF Tinto, Massimo
de Araujo, Jose C. N.
Kuga, Helio K.
Alves, Marcio E. S.
Aguiar, Odylio D.
TI Orbit analysis of a geostationary gravitational wave interferometer
detector array
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
DE gravitational waves; interferometry; geostationary satellites
AB We analyze the trajectories of three geostationary satellites forming the geostationary gravitational wave interferometer (GEOGRAWI) [1], a space-based laser interferometer mission aiming to detect and study gravitational radiation in the (10(-4) -10) Hz band. The combined effects of the gravity fields of the Earth, the Sun and the Moon make the three satellites deviate from their nominally stationary, equatorial and equilateral configuration. Since changes in the satellites's relative distances and orientations could negatively affect the precision of the laser heterodyne measurements, we have derived the time-dependence of the inter-satellite distances and velocities, the variations of the polar angles made by the constellation's three arms with respect to a chosen reference frame and the time changes of the triangle's enclosed angles. We find that during the time between two consecutive station-keeping maneuvers (about two weeks) the relative variations of the inter-satellite distances do not exceed a value of 0.05%, while the relative velocities between pairs of satellites remain smaller than about 0.7 m s(-1). In addition, we find the angles made by the arms of the triangle with the equatorial plane to be periodic functions of time whose amplitudes grow linearly with time; the maximum variations experienced by these angles as well as by those within the triangle remain smaller than 3 arc-minutes, while the east-west angular variations of the three arms remain smaller than about 15 arc-minutes during the two-week period.
C1 [Tinto, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[de Araujo, Jose C. N.; Kuga, Helio K.; Aguiar, Odylio D.] Inst Nacl Pesquisas Espaciais, Sao Jose Dos Campos, SP, Brazil.
[Alves, Marcio E. S.] UNESP Univ Estadual Paulista, Inst Ciencia & Tecnol, Sao Jose Dos Campos, SP, Brazil.
RP Tinto, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM massimo.tinto@jpl.nasa.gov; jcarlos.dearaujo@inpe.br; hkk@dem.inpe.br;
marcio.alves@ict.unesp.br; odylio.aguiar@inpe.br
RI de Araujo, Jose Carlos/C-5181-2013
OI de Araujo, Jose Carlos/0000-0003-4418-4289
FU Jet Propulsion Laboratory Research & Technology Development program;
FAPESP; CNPq; FAPEMIG [APQ-00140-12]
FX M T acknowledges financial support provided by the Jet Propulsion
Laboratory Research & Technology Development program. J C N A thanks
FAPESP and CNPq for partial financial support, while M E S A
acknowledges financial support from FAPEMIG (Grant APQ-00140-12). Last,
but not least, we thank the three anonymous referees for their valuable
comments. For M T, this research was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 21
TC 1
Z9 1
U1 0
U2 2
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 SEP 24
PY 2015
VL 32
IS 18
AR 185017
DI 10.1088/0264-9381/32/18/185017
PG 11
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA CS7NR
UT WOS:000362270800019
ER
PT J
AU Wohl, CJ
Kiefer, JM
Petrosky, BJ
Tiemsin, PI
Lowe, KT
Maisto, PMF
Danehy, PM
AF Wohl, Christopher J.
Kiefer, Jacob M.
Petrosky, Brian J.
Tiemsin, Pacita I.
Lowe, K. Todd
Maisto, Pietro M. F.
Danehy, Paul M.
TI Synthesis of Fluorophore-Doped Polystyrene Microspheres: Seed Material
for Airflow Sensing
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE kiton red 620; PSLs; particle image velocimetry (PIV); emulsifier-free
emulsion polymerization; design of experiments; fluorescent particles
ID DISPERSION POLYMERIZATION; MINIEMULSION POLYMERIZATION; SIZE
DISTRIBUTION; PARTICLE-SIZE; FLUORESCENT; STYRENE; MECHANISM;
DECOMPOSITION; PERSULFATE; ADSORPTION
AB Kiton red 620 (KR620) doped polystyrene latex microspheres (PSLs) were synthesized via soap-free emulsion polymerization to be utilized as a relatively nontoxic, fluorescent seed material for airflow characterization experiments. Poly(styrene-co-styrenesulfonate) was used as the PSL matrix to promote KR620 incorporation. Additionally, a bicarbonate buffer and poly(diallyldimethylammonium chloride), polyD, cationic polymer were added to the reaction solution to stabilize the pH and potentially influence the electrostatic interactions between the PSLs and dye molecules. A design of experiments (DOE) approach was used to efficiently investigate the variation of these materials. Using a 4-factor, 2-level response surface design with a center point, a series of experiments were performed to determine the dependence of these factors on particle diameter, diameter size distribution, fluorescent emission intensity, and KR620 retention. Using statistical analysis, the factors and factor interactions that most significantly affect the outputs were identified. These particles enabled velocity measurements to be made much closer to walls and surfaces than previously. Based on these results, KR620-doped PSLs may be utilized to simultaneously measure the velocity and mixing concentration, among other airflow parameters, in complex flows.
C1 [Wohl, Christopher J.; Tiemsin, Pacita I.; Danehy, Paul M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Kiefer, Jacob M.] NASA, Langley Res Ctr, NASA Langley Res Summer Scholars LARSS, Hampton, VA 23681 USA.
[Petrosky, Brian J.; Lowe, K. Todd; Maisto, Pietro M. F.] Virginia Polytech Inst & State Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24060 USA.
RP Wohl, CJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM c.j.wohl@nasa.gov
FU NASA Aeronautics Research Mission Directorate (ARMD) NASA Aeronautics
Research Institute (NARI)
FX This work was funded by the NASA Aeronautics Research Mission
Directorate (ARMD) NASA Aeronautics Research Institute (NARI) through
Phase 1 and Phase 2 Seedling Projects. We also wish to acknowledge the
work of summer LARSS students Max Verkamp and Brian Koh who contributed
to work leading up to the present study. The authors appreciate the help
of Richard DeLoach from NASA Langley for assisting with the design of
experiments test matrix.
NR 36
TC 1
Z9 1
U1 6
U2 22
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1944-8244
J9 ACS APPL MATER INTER
JI ACS Appl. Mater. Interfaces
PD SEP 23
PY 2015
VL 7
IS 37
BP 20714
EP 20725
DI 10.1021/acsami.5b05584
PG 12
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA CS2WB
UT WOS:000361931600027
PM 26322378
ER
PT J
AU Cooke, EA
Hatch, NA
Rettura, A
Wylezalek, D
Galametz, A
Stern, D
Brodwin, M
Muldrew, SI
Almaini, O
Conselice, CJ
Eisenhardt, PR
Hartley, WG
Jarvis, M
Seymour, N
Stanford, SA
AF Cooke, E. A.
Hatch, N. A.
Rettura, A.
Wylezalek, D.
Galametz, A.
Stern, D.
Brodwin, M.
Muldrew, S. I.
Almaini, O.
Conselice, C. J.
Eisenhardt, P. R.
Hartley, W. G.
Jarvis, M.
Seymour, N.
Stanford, S. A.
TI The formation history of massive cluster galaxies as revealed by CARLA
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: clusters: general; galaxies: evolution; galaxies: formation;
galaxies: high-redshift
ID COLOR-MAGNITUDE RELATION; STELLAR POPULATION SYNTHESIS; STAR-FORMATION
HISTORIES; LESS-THAN 3.2; TP-AGB STARS; LUMINOSITY FUNCTION;
HIGH-REDSHIFT; RED SEQUENCE; RADIO GALAXY; DISTANT CLUSTERS
AB We use a sample of 37 of the densest clusters and protoclusters across 1.3 = z = 3.2 from the Clusters Around Radio-Loud AGN (CARLA) survey to study the formation of massive cluster galaxies. We use optical i'band and infrared 3.6 and 4.5 mu m images to statistically select sources within these protoclusters and measure their median observed colours; < i' - [3.6]>. We find the abundance of massive galaxies within the protoclusters increases with decreasing redshift, suggesting these objects may form an evolutionary sequence, with the lower redshift clusters in the sample having similar properties to the descendants of the high-redshift protoclusters. We find that the protocluster galaxies have an approximately unevolving observed-frame i' - [3.6] colour across the examined redshift range. We compare the evolution of the < i' - [3.6]> colour of massive cluster galaxies with simplistic galaxy formation models. Taking the full cluster population into account, we show that the formation of stars within the majority of massive cluster galaxies occurs over at least 2 Gyr, and peaks at z similar to 2-3. From the median i' - [3.6] colours, we cannot determine the star formation histories of individual galaxies, but their star formation must have been rapidly terminated to produce the observed red colours. Finally, we show that massive galaxies at z > 2 must have assembled within 0.5 Gyr of them forming a significant fraction of their stars. This means that few massive galaxies in z > 2 protoclusters could have formed via dry mergers.
C1 [Cooke, E. A.; Hatch, N. A.; Almaini, O.; Conselice, C. J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Rettura, A.; Stern, D.; Eisenhardt, P. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Rettura, A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Wylezalek, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Galametz, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Brodwin, M.] UMKC Dept Phys & Astron, Kansas City, MO 64110 USA.
[Muldrew, S. I.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Hartley, W. G.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Jarvis, M.] Univ Oxford, Astrophys, Oxford OX1 3RH, England.
[Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa.
[Seymour, N.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
RP Cooke, EA (reprint author), Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England.
EM Elizabeth.Cooke@nottingham.ac.uk
OI Hatch, Nina/0000-0001-5600-0534; Seymour, Nicholas/0000-0003-3506-5536;
Almaini, Omar/0000-0001-9328-3991
FU STFC; STFC Rutherford Fellowship; STFC consolidated grant
[ST/K001000/1]; ARC Future Fellowship; William Herschel Telescope
[W/2013b/10, W/2014a/6, SW/2013b/34]; Gemini Observatory
[GS-2014A-Q-45]; NASA through JPL/Caltech
FX EAC acknowledges support from the STFC. NAH is supported by an STFC
Rutherford Fellowship. The work of DS was carried out at Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA. SIM acknowledges the support of the STFC consolidated grant
(ST/K001000/1). NS is the recipient of an ARC Future Fellowship.; Based
on observations made with the William Herschel Telescope under programme
IDs W/2013b/10, W/2014a/6 and SW/2013b/34, and the Gemini Observatory
under programme ID GS-2014A-Q-45. The William Herschel Telescope
operates 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 is based on observations made with
the Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. Support for this work was provided by NASA through an award issued
by JPL/Caltech.
NR 78
TC 5
Z9 5
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 21
PY 2015
VL 452
IS 3
BP 2318
EP 2336
DI 10.1093/mnras/stv1413
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8JQ
UT WOS:000360854200008
ER
PT J
AU Giocoli, C
Metcalf, RB
Baldi, M
Meneghetti, M
Moscardini, L
Petkova, M
AF Giocoli, Carlo
Metcalf, R. Benton
Baldi, Marco
Meneghetti, Massimo
Moscardini, Lauro
Petkova, Margarita
TI Disentangling dark sector models using weak lensing statistics
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; methods: numerical; galaxies: haloes;
cosmology: theory; dark matter
ID HUBBLE-SPACE-TELESCOPE; N-BODY SIMULATIONS; GALAXY CLUSTERS; ENERGY
COSMOLOGIES; COSMIC SHEAR; POWER SPECTRUM; MASS; MATTER; CFHTLENS;
UNIVERSE
AB We perform multiplane ray tracing using the GLAMER gravitational lensing code within high-resolution light-cones extracted from the CoDECS simulations: a suite of cosmological runs featuring a coupling between dark energy and cold dark matter (CDM). We show that the presence of the coupling is evident not only in the redshift evolution of the normalization of the convergence power spectrum, but also in differences in non-linear structure formation with respect to Lambda CDM. Using a tomographic approach under the assumption of a Lambda CDM cosmology, we demonstrate that weak lensing measurements would result in a sigma(8) value that changes with the source redshift if the true underlying cosmology is a coupled dark energy (cDE) one. This provides a generic null test for these types of models. We also find that different models of cDE can show either an enhanced or a suppressed correlation between convergence maps with differing source redshifts as compared to Lambda CDM. This would provide a direct way to discriminate between different possible realizations of the cDE scenario. Finally, we discuss the impact of the coupling on several lensing observables for different source redshifts and angular scales with realistic source redshift distributions for current ground-based and future space-based lensing surveys.
C1 [Giocoli, Carlo; Metcalf, R. Benton; Baldi, Marco; Moscardini, Lauro] Univ Bologna, Alma Mater Studiorum, Dipartimento Fis & Astron, I-40127 Bologna, Italy.
[Giocoli, Carlo; Baldi, Marco; Meneghetti, Massimo; Moscardini, Lauro] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Giocoli, Carlo; Baldi, Marco; Meneghetti, Massimo; Moscardini, Lauro] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy.
[Giocoli, Carlo] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Meneghetti, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Petkova, Margarita] Univ Munich, Dept Phys, D-81679 Munich, Germany.
RP Giocoli, C (reprint author), Univ Bologna, Alma Mater Studiorum, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
EM carlo.giocoli@lam.fr
RI Meneghetti, Massimo/O-8139-2015;
OI Meneghetti, Massimo/0000-0003-1225-7084; METCALF, ROBERT
BENTON/0000-0003-3167-2574
FU CNES; European Seventh Framework Programme, Ideas [259349]; Marie Curie
Intra European Fellowship 'SIDUN' within the 7th Framework Programme of
the European Commission; PRIN MIUR; PRIN INAF; [ASI/INAF I/023/12/0]
FX We thank the anonymous referee for her/his useful comments that help to
improve the presentation of our results. CG thanks CNES for its
financial support. CG and RBM's research is part of the project GLENCO,
funded under the European Seventh Framework Programme, Ideas, Grant
Agreement n. 259349. MB acknowledges support by the Marie Curie Intra
European Fellowship 'SIDUN' within the 7th Framework Programme of the
European Commission. We acknowledge financial contributions from
contracts ASI/INAF I/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, MB and LM also acknowledge the financial contribution by
the PRIN INAF 2012 'The Universe in the box: multiscale simulations of
cosmic structure'. We also thank Cosimo Fedeli, Federico Marulli,
Michele Moresco and Mauro Roncarelli for useful discussions. GC thank
Giulia Despali, Giuseppe Tormen and Vincenzo Mezzalira to have host part
of the computer jobs run to perform the ray tracing.
NR 94
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U1 0
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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 SEP 21
PY 2015
VL 452
IS 3
BP 2757
EP 2772
DI 10.1093/mnras/stv1473
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8JQ
UT WOS:000360854200040
ER
PT J
AU Yuan, F
Lidman, C
Davis, TM
Childress, M
Abdalla, FB
Banerji, M
Buckley-Geer, E
Rosell, AC
Carollo, D
Castander, FJ
D'Andrea, CB
Diehl, HT
Cunha, CE
Foley, RJ
Frieman, J
Glazebrook, K
Gschwend, J
Hinton, S
Jouvel, S
Kessler, R
Kim, AG
King, AL
Kuehn, K
Kuhlmann, S
Lewis, GF
Lin, H
Martini, P
McMahon, RG
Mould, J
Nichol, RC
Norris, RP
O'Neill, CR
Ostrovski, F
Papadopoulos, A
Parkinson, D
Reed, S
Romer, AK
Rooney, PJ
Rozo, E
Rykoff, ES
Sako, M
Scalzo, R
Schmidt, BP
Scolnic, D
Seymour, N
Sharp, R
Sobreira, F
Sullivan, M
Thomas, RC
Tucker, D
Uddin, SA
Wechsler, RH
Wester, W
Wilcox, H
Zhang, B
Abbott, T
Allam, S
Bauer, AH
Benoit-Levy, A
Bertin, E
Brooks, D
Burke, DL
Kind, MC
Covarrubias, R
Crocce, M
da Costa, LN
Depoy, DL
Desai, S
Doel, P
Eifler, TF
Evrard, AE
Neto, A
Flaugher, B
Fosalba, P
Gaztanaga, E
Gerdes, D
Gruen, D
Gruendl, RA
Honscheid, K
James, D
Kuropatkin, N
Lahav, O
Li, TS
Maia, MAG
Makler, M
Marshall, J
Miller, CJ
Miquel, R
Ogando, R
Plazas, AA
Roodman, A
Sanchez, E
Scarpine, V
Schubnell, M
Sevilla-Noarbe, I
Smith, RC
Soares-Santos, M
Suchyta, E
Swanson, MEC
Tarle, G
Thaler, J
Walker, AR
AF Yuan, Fang
Lidman, C.
Davis, T. M.
Childress, M.
Abdalla, F. B.
Banerji, M.
Buckley-Geer, E.
Carnero Rosell, A.
Carollo, D.
Castander, F. J.
D'Andrea, C. B.
Diehl, H. T.
Cunha, C. E.
Foley, R. J.
Frieman, J.
Glazebrook, K.
Gschwend, J.
Hinton, S.
Jouvel, S.
Kessler, R.
Kim, A. G.
King, A. L.
Kuehn, K.
Kuhlmann, S.
Lewis, G. F.
Lin, H.
Martini, P.
McMahon, R. G.
Mould, J.
Nichol, R. C.
Norris, R. P.
O'Neill, C. R.
Ostrovski, F.
Papadopoulos, A.
Parkinson, D.
Reed, S.
Romer, A. K.
Rooney, P. J.
Rozo, E.
Rykoff, E. S.
Sako, M.
Scalzo, R.
Schmidt, B. P.
Scolnic, D.
Seymour, N.
Sharp, R.
Sobreira, F.
Sullivan, M.
Thomas, R. C.
Tucker, D.
Uddin, S. A.
Wechsler, R. H.
Wester, W.
Wilcox, H.
Zhang, B.
Abbott, T.
Allam, S.
Bauer, A. H.
Benoit-Levy, A.
Bertin, E.
Brooks, D.
Burke, D. L.
Kind, M. Carrasco
Covarrubias, R.
Crocce, M.
da Costa, L. N.
DePoy, D. L.
Desai, S.
Doel, P.
Eifler, T. F.
Evrard, A. E.
Fausti Neto, A.
Flaugher, B.
Fosalba, P.
Gaztanaga, E.
Gerdes, D.
Gruen, D.
Gruendl, R. A.
Honscheid, K.
James, D.
Kuropatkin, N.
Lahav, O.
Li, T. S.
Maia, M. A. G.
Makler, M.
Marshall, J.
Miller, C. J.
Miquel, R.
Ogando, R.
Plazas, A. A.
Roodman, A.
Sanchez, E.
Scarpine, V.
Schubnell, M.
Sevilla-Noarbe, I.
Smith, R. C.
Soares-Santos, M.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Thaler, J.
Walker, A. R.
TI OzDES multifibre spectroscopy for the Dark Energy Survey: first-year
operation and results
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: spectroscopic; surveys; supernovae: general; galaxies:
active; cosmology: observations
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SUPERNOVA LEGACY SURVEY;
BLACK-HOLE MASS; INFRARED EXTRAGALACTIC FIELD; IA SUPERNOVAE; HOST
GALAXIES; RADIO OBSERVATIONS; HUBBLE RESIDUALS; STAR-FORMATION
AB The Australian Dark Energy Survey (OzDES) is a five-year, 100-night, spectroscopic survey on the Anglo-Australian Telescope, whose primary aim is to measure redshifts of approximately 2500 Type Ia supernovae host galaxies over the redshift range 0.1 < z < 1.2, and derive reverberation-mapped black hole masses for approximately 500 active galactic nuclei and quasars over 0.3 < z < 4.5. This treasure trove of data forms a major part of the spectroscopic follow-up for the Dark Energy Survey for which we are also targeting cluster galaxies, radio galaxies, strong lenses, and unidentified transients, as well as measuring luminous red galaxies and emission line galaxies to help calibrate photometric redshifts. Here, we present an overview of the OzDES programme and our first-year results. Between 2012 December and 2013 December, we observed over 10 000 objects and measured more than 6 000 redshifts. Our strategy of retargeting faint objects across many observing runs has allowed us to measure redshifts for galaxies as faint as m(r) = 25 mag. We outline our target selection and observing strategy, quantify the redshift success rate for different types of targets, and discuss the implications for our main science goals. Finally, we highlight a few interesting objects as examples of the fortuitous yet not totally unexpected discoveries that can come from such a large spectroscopic survey.
C1 [Yuan, Fang; Childress, M.; Scalzo, R.; Schmidt, B. P.; Sharp, R.; Zhang, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Yuan, Fang; Lidman, C.; Davis, T. M.; Childress, M.; Hinton, S.; O'Neill, C. R.; Scalzo, R.; Schmidt, B. P.; Uddin, S. A.; Zhang, B.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW, Australia.
[Lidman, C.; Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Davis, T. M.; Hinton, S.; King, A. L.; O'Neill, C. R.; Parkinson, D.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia.
[Abdalla, F. B.; Jouvel, S.; Benoit-Levy, A.; Brooks, D.; Doel, P.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Banerji, M.; McMahon, R. G.; Ostrovski, F.; Reed, S.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England.
[Banerji, M.; McMahon, R. G.; Ostrovski, F.; Reed, S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Buckley-Geer, E.; Diehl, H. T.; Frieman, J.; Lin, H.; Sobreira, F.; Tucker, D.; Wester, W.; Allam, S.; Flaugher, B.; Kuropatkin, N.; Scarpine, V.; Soares-Santos, M.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Carnero Rosell, A.; Gschwend, J.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Carnero Rosell, A.; Gschwend, J.; Sobreira, F.; da Costa, L. N.; Fausti Neto, A.; Maia, M. A. G.; Ogando, R.] Lab Interinst & Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Carollo, D.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Carollo, D.] Univ Notre Dame, JINA Ctr Evolut Elements, Notre Dame, IN 46556 USA.
[Carollo, D.] INAF, Astrophys Observ Turin, I-10025 Pino Torinese, Italy.
[Castander, F. J.; Bauer, A. H.; Crocce, M.; Fosalba, P.; Gaztanaga, E.] CSIC, Fac Ciencies, IEEC, Inst Ciencies Espai, E-08193 Barcelona, Spain.
[D'Andrea, C. B.; Nichol, R. C.; Papadopoulos, A.; Wilcox, H.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Cunha, C. E.; Wechsler, R. H.; Burke, D. L.; Roodman, A.] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Foley, R. J.; Kind, M. Carrasco; Gruendl, R. A.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Foley, R. J.; Thaler, J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Frieman, J.; Kessler, R.; Scolnic, D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Glazebrook, K.; Mould, J.; Uddin, S. A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Kim, A. G.; Thomas, R. C.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[King, A. L.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Kuhlmann, S.] Argonne Natl Lab, Lemont, IL 60439 USA.
[Lewis, G. F.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Martini, P.; Honscheid, K.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Martini, P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Norris, R. P.] CSIRO, Astron & Space Sci, Epping, NSW 1710, Australia.
[Ostrovski, F.] Minist Educ Brazil, CAPES Fdn, BR-70040020 Brasilia, DF, Brazil.
[Romer, A. K.; Rooney, P. J.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Rozo, E.; Rykoff, E. S.; Wechsler, R. H.; Burke, D. L.; Roodman, A.] SLAC, Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA.
[Sako, M.; Eifler, T. F.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Seymour, N.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Sullivan, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Wechsler, R. H.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Abbott, T.; James, D.; Smith, R. C.; Walker, A. R.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile.
[Bertin, E.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France.
[Bertin, E.] CNRS, UMR7095, F-75014 Paris, France.
[Kind, M. Carrasco; Covarrubias, R.; Gruendl, R. A.; Swanson, M. E. C.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[DePoy, D. L.; Li, T. S.; Marshall, J.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[DePoy, D. L.; Li, T. S.; Marshall, J.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Desai, S.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Evrard, A. E.; Gerdes, D.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Gruen, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
Univ Observ Munich, D-81679 Munich, Germany.
[Honscheid, K.; Suchyta, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Makler, M.] Ctr Brasileiro Pesquisas Fis, ICRA, BR-22290 Rio De Janeiro, RJ, Brazil.
[Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
[Plazas, A. A.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Sanchez, E.; Sevilla-Noarbe, I.] CIEMAT, E-28040 Madrid, Spain.
RP Yuan, F (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
EM fang.yuan@anu.edu.au
RI Ogando, Ricardo/A-1747-2010; Glazebrook, Karl/N-3488-2015; Makler,
Martin/G-2639-2012; Sanchez, Eusebio/H-5228-2015; Fosalba Vela,
Pablo/I-5515-2016; Sobreira, Flavia/F-4168-2015; Parkinson,
David/E-1183-2013; Davis, Tamara/A-4280-2008; Gaztanaga,
Enrique/L-4894-2014;
OI Suchyta, Eric/0000-0002-7047-9358; Seymour,
Nicholas/0000-0003-3506-5536; Norris, Ray/0000-0002-4597-1906; Schmidt,
Brian/0000-0001-6589-1287; McMahon, Richard/0000-0001-8447-8869;
Banerji, Manda/0000-0002-0639-5141; Scalzo, Richard/0000-0003-3740-1214;
Abdalla, Filipe/0000-0003-2063-4345; Sullivan, Mark/0000-0001-9053-4820;
Yuan, Fang/0000-0001-8315-4176; Ogando, Ricardo/0000-0003-2120-1154;
Glazebrook, Karl/0000-0002-3254-9044; Makler,
Martin/0000-0003-2206-2651; Sanchez, Eusebio/0000-0002-9646-8198;
Sobreira, Flavia/0000-0002-7822-0658; Parkinson,
David/0000-0002-7464-2351; Davis, Tamara/0000-0002-4213-8783; Gaztanaga,
Enrique/0000-0001-9632-0815; Reed, Sophie/0000-0002-4422-0553; Carrasco
Kind, Matias/0000-0002-4802-3194; Tucker, Douglas/0000-0001-7211-5729
FU Australian Research Council Centre of Excellence for All-sky
Astrophysics (CAASTRO) [CE110001020]; PAPDRJ CAPES/FAPERJ Fellowship; US
Department of Energy [DE-AC02-76SF00515]; Australian Research Council
Laureate Fellowship [LF0992131]; Australian Research Council Future
Fellowship; CAPES [3171-13-2]; Australian Astronomical Observatory (AAO)
[A/2012B/11, A/2013B/12, NOAO/0278]; US Department of Energy; US
National Science Foundation; Ministry of Science and Education of Spain;
Science and Technology Facilities Council of the United Kingdom; Higher
Education Funding Council for England; National Center for
Supercomputing Applications at the University of Illinois at
Urbana-Champaign; Kavli Institute of Cosmological Physics at the
University of Chicago; Center for Cosmology and Astro-Particle Physics
at the Ohio State University; Mitchell Institute for Fundamental Physics
and Astronomy at Texas AM University; Financiadora de Estudos e
Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do
Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e
Tecnologico; Ministerio da Ciencia e Tecnologia; Deutsche
Forschungsgemeinschaft; Dark Energy Survey; National Science Foundation
[AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986];
Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Union;
Argonne National Laboratory; University of California at Santa Cruz;
University of Cambridge; Centro de Investigaciones Energeticas;
Medioambientales y Tecnologicas-Madrid; University of Chicago;
University College London; DES-Brazil Consortium; Eidgenossische
Technische Hochschule (ETH) Zurich; Fermi National Accelerator
Laboratory; University of Edinburgh; University of Illinois at
Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut
de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory;
Ludwig-Maximilians Universitat; associated Excellence Cluster Universe;
University of Michigan; National Optical Astronomy Observatory;
University of Nottingham; The Ohio State University; University of
Pennsylvania; University of Portsmouth; SLAC National Accelerator
Laboratory; Stanford University; University of Sussex; Texas AM
University
FX Parts of this research were conducted by the Australian Research Council
Centre of Excellence for All-sky Astrophysics (CAASTRO), through project
number CE110001020. ACR acknowledges financial support provided by the
PAPDRJ CAPES/FAPERJ Fellowship. This work was supported in part by the
US Department of Energy contract to SLAC No. DE-AC02-76SF00515. BPS
acknowledges support from the Australian Research Council Laureate
Fellowship Grant LF0992131. NS is the recipient of an Australian
Research Council Future Fellowship. FS acknowledges financial support
provided by CAPES under contract No. 3171-13-2; The data in this paper
were based on observations obtained at the Australian Astronomical
Observatory (AAO programs A/2012B/11 and A/2013B/12, and NOAO program
NOAO/0278). The authors would like to thank Marguerite Pierre and the
XMM-XXL collaboration for allowing them to use a couple of hours of
their time on the AAT to target the DES C3 field.; Funding for the DES
Projects has been provided by the US Department of Energy, the US
National Science Foundation, the Ministry of Science and Education of
Spain, the Science and Technology Facilities Council of the United
Kingdom, the Higher Education Funding Council for England, the National
Center for Supercomputing Applications at the University of Illinois at
Urbana-Champaign, the Kavli Institute of Cosmological Physics at the
University of Chicago, the Center for Cosmology and Astro-Particle
Physics at the Ohio State University, the Mitchell Institute for
Fundamental Physics and Astronomy at Texas A&M University, Financiadora
de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa
do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento
Cientifico e Tecnologico and the Ministerio da Ciencia e Tecnologia, the
Deutsche Forschungsgemeinschaft and the Collaborating Institutions in
the Dark Energy Survey.; The DES data management system is supported by
the National Science Foundation under Grant Number AST-1138766. The DES
participants from Spanish institutions are partially supported by MINECO
under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de
Excelencia Severo Ochoa SEV-2012-0234, some of which include ERDF funds
from the European Union.; The Collaborating Institutions are Argonne
National Laboratory, the University of California at Santa Cruz, the
University of Cambridge, Centro de Investigaciones Energeticas,
Medioambientales y Tecnologicas-Madrid, the University of Chicago,
University College London, the DES-Brazil Consortium, the Eidgenossische
Technische Hochschule (ETH) Zurich, Fermi National Accelerator
Laboratory, the University of Edinburgh, the University of Illinois at
Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the
Institut de Fisica d'Altes Energies, Lawrence Berkeley National
Laboratory, the Ludwig-Maximilians Universitat and the associated
Excellence Cluster Universe, the University of Michigan, the National
Optical Astronomy Observatory, the University of Nottingham, The Ohio
State University, the University of Pennsylvania, the University of
Portsmouth, SLAC National Accelerator Laboratory, Stanford University,
the University of Sussex, and Texas A&M University.
NR 64
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U1 2
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 SEP 21
PY 2015
VL 452
IS 3
BP 3047
EP 3063
DI 10.1093/mnras/stv1507
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8JQ
UT WOS:000360854200062
ER
PT J
AU Ursini, F
Marinucci, A
Matt, G
Bianchi, S
Tortosa, A
Stern, D
Arevalo, P
Ballantyne, DR
Bauer, FE
Fabian, AC
Harrison, FA
Lohfink, AM
Reynolds, CS
Walton, DJ
AF Ursini, F.
Marinucci, A.
Matt, G.
Bianchi, S.
Tortosa, A.
Stern, D.
Arevalo, P.
Ballantyne, D. R.
Bauer, F. E.
Fabian, A. C.
Harrison, F. A.
Lohfink, A. M.
Reynolds, C. S.
Walton, D. J.
TI The NuSTAR X-ray spectrum of the low-luminosity active galactic nucleus
in NGC 7213
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: individual: NGC 7213; galaxies: Seyfert;
X-rays: galaxies
ID K-ALPHA LINE; BLACK-HOLE MASS; ADVECTION-DOMINATED ACCRETION;
SEYFERT-GALAXIES; ULTRAVIOLET EMISSION; XMM-NEWTON; COMPTON REFLECTION;
NEARBY GALAXIES; CORONA MODEL; NGC-7213
AB We present an analysis of the 3-79 keV NuSTAR spectrum of the low-luminosity active galactic nucleus NGC 7213. In agreement with past observations, we find a lower limit to the high-energy cut-off of E-c > 140 keV, no evidence for a Compton-reflected continuum and the presence of an iron K alpha complex, possibly produced in the broad-line region. From the application of the MYTORUS model, we find that the line-emitting material is consistent with the absence of a significant Compton reflection if arising from a Compton-thin torus of gas with a column density of 5.0(-1.6)(+2.0) x 10(23) cm(-2). We report variability of the equivalent width of the iron lines on the time-scale of years using archival observations from XMM-Newton, Chandra and Suzaku. This analysis suggests a possible contribution from dusty gas. A fit with a Comptonization model indicates the presence of a hot corona with a temperature kT(e) > 40 keV and an optical depth tau less than or similar to 1, assuming a spherical geometry.
C1 [Ursini, F.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Ursini, F.] CNRS, IPAG, F-38000 Grenoble, France.
[Ursini, F.; Marinucci, A.; Matt, G.; Bianchi, S.; Tortosa, A.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
[Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso 2360102, Chile.
[Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Millennium Inst Astrophys, Macul 7820436, Santiago, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Fabian, A. C.; Lohfink, A. M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Reynolds, C. S.] Joint Space Sci Inst JSI, College Pk, MD 20742 USA.
[Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RP Ursini, F (reprint author), Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
EM francesco.ursini@obs.ujf-grenoble.fr
RI Bianchi, Stefano/B-4804-2010; XRAY, SUZAKU/A-1808-2009
OI Bianchi, Stefano/0000-0002-4622-4240;
FU NASA; French-Italian International Project of Scientific Collaboration:
PICS-INAF [181542]; CNES; Universite Franco-Italienne (Vinci PhD
fellowship); Italian Space Agency [ASI/INAF I/037/12/0-011/13, ASI-INAF
I/037/12/P1]; FONDECYT [1140304]; CONICYT-Chile [PFB-06/2007, 1141218,
ACT1101]; Ministry of Economy, Development, and Tourism's Millennium
Science Initiative [IC120009]
FX We thank the anonymous referee for his/her helpful comments, which
improved the manuscript. FU thanks Pierre-Olivier Petrucci for useful
discussions and comments. This work is based on observations obtained
with the NuSTAR mission, a project led by the California Institute of
Technology, managed by the Jet Propulsion Laboratory and funded by NASA.
This research has made use of data, software and/or web tools obtained
from NASA's High Energy Astrophysics Science Archive Research Center
(HEASARC), a service of Goddard Space Flight Center and the Smithsonian
Astrophysical Observatory. FU, GM and SB acknowledge support from the
French-Italian International Project of Scientific Collaboration:
PICS-INAF project number 181542. FU acknowledges support from CNES and
Universite Franco-Italienne (Vinci PhD fellowship). FU, AM and GM
acknowledge financial support from the Italian Space Agency under grant
ASI/INAF I/037/12/0-011/13. SB acknowledges financial support from the
Italian Space Agency under grant ASI-INAF I/037/12/P1. PA acknowledges
support from FONDECYT 1140304. FEB acknowledges support from
CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, 'EMBIGGEN'
Anillo ACT1101) and the Ministry of Economy, Development, and Tourism's
Millennium Science Initiative through grant IC120009, awarded to The
Millennium Institute of Astrophysics, MAS.
NR 73
TC 8
Z9 8
U1 1
U2 6
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 21
PY 2015
VL 452
IS 3
BP 3266
EP 3272
DI 10.1093/mnras/stv1527
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8JQ
UT WOS:000360854200079
ER
PT J
AU Caspi, A
Shih, AY
McTiernan, JM
Krucker, S
AF Caspi, Amir
Shih, Albert Y.
McTiernan, James M.
Krucker, Saem
TI HARD X-RAY IMAGING OF INDIVIDUAL SPECTRAL COMPONENTS IN SOLAR FLARES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE methods: data analysis; plasmas; radiation mechanisms: thermal; Sun:
corona; Sun: flares; Sun: X-rays, gamma rays
ID DIFFERENTIAL EMISSION MEASURES; ACTIVE REGIONS; RHESSI; ACCELERATION;
VISIBILITIES; ELECTRONS; PLASMA; SDO
AB We present a new analytical technique, combining Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) high-resolution imaging and spectroscopic observations, to visualize solar flare emission as a function of spectral component (e.g., isothermal temperature) rather than energy. This computationally inexpensive technique is applicable to all spatially invariant spectral forms and is useful for visualizing spectroscopically determined individual sources and placing them in context, e.g., comparing multiple isothermal sources with nonthermal emission locations. For example, while extreme ultraviolet images can usually be closely identified with narrow temperature ranges, due to the emission being primarily from spectral lines of specific ion species, X-ray images are dominated by continuum emission and therefore have a broad temperature response, making it difficult to identify sources of specific temperatures regardless of the energy band of the image. We combine RHESSI calibrated X-ray visibilities with spatially integrated spectral models including multiple isothermal components to effectively isolate the individual thermal sources from the combined emission and image them separately. We apply this technique to the 2002 July 23 X4.8 event studied in prior works, and image for the first time the super-hot and cooler thermal sources independently. The super-hot source is farther from the footpoints and more elongated throughout the impulsive phase, consistent with an in situ heating mechanism for the super-hot plasma.
C1 [Caspi, Amir] SW Res Inst, Boulder, CO 80302 USA.
[Shih, Albert Y.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[McTiernan, James M.; Krucker, Saem] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Krucker, Saem] Univ Appl Sci & Arts Northwestern Switzerland, Sch Engn, Inst Technol 4D, CH-5210 Windisch, Switzerland.
RP Caspi, A (reprint author), SW Res Inst, Boulder, CO 80302 USA.
OI Caspi, Amir/0000-0001-8702-8273
FU NASA [NAS5-98033, NNX08AJ18G, NNX12AH48G]
FX This work was supported by NASA contract NAS5-98033. A.C. and J.M.M.
were also supported by NASA grants NNX08AJ18G and NNX12AH48G. We thank
G. Hurford and R. Schwartz for many helpful discussions.
NR 27
TC 2
Z9 2
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 SEP 20
PY 2015
VL 811
IS 1
AR L1
DI 10.1088/2041-8205/811/1/L1
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CV5VY
UT WOS:000364340600001
ER
PT J
AU Pasham, DR
Cenko, SB
Zoghbi, A
Mushotzky, RF
Miller, J
Tombesi, F
AF Pasham, Dheeraj R.
Cenko, S. Bradley
Zoghbi, Abderahmen
Mushotzky, Richard F.
Miller, Jon
Tombesi, Francesco
TI EVIDENCE FOR HIGH-FREQUENCY QPOs WITH A 3:2 FREQUENCY RATIO FROM A 5000
SOLAR MASS BLACK HOLE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE black hole physics; methods: data analysis; X-rays: binaries; X-rays:
individual (NGC 1313 X-1)
ID X-RAY SOURCES; QUASI-PERIODIC OSCILLATIONS; NGC 5408 X-1; MICROQUASAR
XTE J1550-564; HIGH-RESOLUTION CAMERA; COOL ACCRETION DISKS; GRO
J1655-40; XMM-NEWTON; GALAXY M82; DISCOVERY
AB Following the discovery of 3:2 resonance quasi-periodic oscillations (QPOs) in M82X-1, we have constructed power density spectra (PDS) of all 15 (sufficiently long) XMM-Newton observations of the ultraluminous X-ray source NGC 1313 X-1 (L-X approximate to 2 x 10(40) erg s(-1)). We detect a strong QPO at a frequency of 0.29 +/- 0.01 Hz in data obtained on 2012 December 16. Subsequent searching of all the remaining observations for a 3:2/2:3 frequency pair revealed a feature at 0.46 +/- 0.02 Hz on 2003 December 13 (frequency ratio of 1.59 +/- 0.09). The global significance of the 0.29 Hz feature considering all frequencies between 0.1 and 4 Hz is >3.5 sigma. The significance of the 0.46 +/- 0.02 Hz QPO is >3.5 sigma for a search at 2/3 and 3/2 of 0.29 Hz. We also detect lower-frequency QPOs (32.9 +/- 2.6 and 79.7 +/- 1.2 mHz). All the QPOs are superimposed on a continuum consisting of flat-topped, band-limited noise, breaking into a power law at a frequency of 16 +/- 3 mHz and white noise at greater than or similar to 0.1 Hz. NGC 1313 X-1's PDS is analogous to stellar-mass black holes' (StMBHs) PDS in the so-called steep power-law state, but with the respective frequencies (both QPOs and break frequencies) scaled down by a factor of similar to 1000. Using the inverse mass-to-high-frequency QPO scaling of StMBHs, we estimate NGC 1313 X-1's black hole mass to be 5000 +/- 1300 M-circle dot, consistent with an inference from the scaling of the break frequency. However, the implied Eddington ratio, L-Edd > 0.03 +/- 0.01, is significantly lower compared to that of StMBHs in the steep power-law state (L-Edd greater than or similar to 0.2).
C1 [Pasham, Dheeraj R.; Cenko, S. Bradley; Mushotzky, Richard F.; Tombesi, Francesco] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Pasham, Dheeraj R.; Cenko, S. Bradley; Tombesi, Francesco] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Pasham, Dheeraj R.; Cenko, S. Bradley; Mushotzky, Richard F.; Tombesi, Francesco] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Zoghbi, Abderahmen; Miller, Jon] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Zoghbi, Abderahmen] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
RP Pasham, DR (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
EM dheerajrangareddy.pasham@nasa.gov; brad.cenko@nasa.gov;
abzoghbi@umich.edu; richard@astro.umd.edu; jonmm@umich.edu;
ftombesi@astro.umd.edu
RI Zoghbi, Abderahmen/A-8445-2017
OI Zoghbi, Abderahmen/0000-0002-0572-9613
NR 44
TC 3
Z9 3
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 SEP 20
PY 2015
VL 811
IS 1
AR L11
DI 10.1088/2041-8205/811/1/L11
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CV5VY
UT WOS:000364340600011
ER
PT J
AU Wang, TJ
Ofman, L
Sun, XD
Provornikova, E
Davila, JM
AF Wang, Tongjiang
Ofman, Leon
Sun, Xudong
Provornikova, Elena
Davila, Joseph M.
TI EVIDENCE OF THERMAL CONDUCTION SUPPRESSION IN A SOLAR FLARING LOOP BY
CORONAL SEISMOLOGY OF SLOW-MODE WAVES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: corona; Sun: flares; Sun: oscillations; Sun: UV radiation; waves
ID STEEP TEMPERATURE-GRADIENTS; X-RAY TELESCOPE; NUMERICAL SIMULATIONS;
MAGNETIC-FIELD; HEAT-TRANSPORT; OSCILLATIONS; SUMER; FLARES;
RECONNECTION; HINODE/EIS
AB Analysis of a longitudinal wave event observed by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory is presented. A time sequence of 131 angstrom images reveals that a C-class flare occurred at one footpoint of a large loop and triggered an intensity disturbance (enhancement) propagating along it. The spatial features and temporal evolution suggest that a fundamental standing slow-mode wave could be set up quickly after meeting of two initial disturbances from the opposite footpoints. The oscillations have a period of similar to 12 minutes and a decay time of similar to 9 minutes. The measured phase speed of 500 +/- 50 km s(-1) matches the sound speed in the heated loop of similar to 10 MK, confirming that the observed waves are of slow mode. We derive the time-dependent temperature and electron density wave signals from six AIA extreme-ultraviolet channels, and find that they are nearly in phase. The measured polytropic index from the temperature and density perturbations is 1.64 +/- 0.08 close to the adiabatic index of 5/3 for an ideal monatomic gas. The interpretation based on a 1D linear MHD model suggests that the thermal conductivity is suppressed by at least a factor of 3 in the hot flare loop at 9MK and above. The viscosity coefficient is determined by coronal seismology from the observed wave when only considering the compressive viscosity dissipation. We find that to interpret the rapid wave damping, the classical compressive viscosity coefficient needs to be enhanced by a factor of 15 as the upper limit.
C1 [Wang, Tongjiang; Ofman, Leon; Provornikova, Elena] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wang, Tongjiang; Ofman, Leon; Provornikova, Elena; Davila, Joseph M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Ofman, Leon] Tel Aviv Univ, Dept Geosci, IL-69978 Tel Aviv, Israel.
[Sun, Xudong] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
RP Wang, TJ (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave NE, Washington, DC 20064 USA.
EM tongjiang.wang@nasa.gov
RI Sun, Xudong/M-3245-2013
OI Sun, Xudong/0000-0003-4043-616X
FU NASA [NNX12AB34G, NNG11PL10A]
FX The work of T.W. was supported by NASA grants NNX12AB34G and the NASA
Cooperative Agreement NNG11PL10A to CUA. L.O. and E.P. acknowledge
support from NASA grant NNX12AB34G. SDO is a mission for NASAs Living
With a Star (LWS) program.
NR 47
TC 0
Z9 0
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2015
VL 811
IS 1
AR L13
DI 10.1088/2041-8205/811/1/L13
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CV5VY
UT WOS:000364340600013
ER
PT J
AU Whitaker, KE
Franx, M
Bezanson, R
Brammer, GB
van Dokkum, PG
Kriek, MT
Labbe, I
Leja, J
Momcheva, IG
Nelson, EJ
Rigby, JR
Rix, HW
Skelton, RE
van der Wel, A
Wuyts, S
AF Whitaker, Katherine E.
Franx, Marijn
Bezanson, Rachel
Brammer, Gabriel B.
van Dokkum, Pieter G.
Kriek, Mariska T.
Labbe, Ivo
Leja, Joel
Momcheva, Ivelina G.
Nelson, Erica J.
Rigby, Jane R.
Rix, Hans-Walter
Skelton, Rosalind E.
van der Wel, Arjen
Wuyts, Stijn
TI GALAXY STRUCTURE AS A DRIVER OF THE STAR FORMATION SEQUENCE SLOPE AND
SCATTER
SO Astrophysical Journal Letters
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift
ID HUBBLE-SPACE-TELESCOPE; EXTRAGALACTIC LEGACY SURVEY; STELLAR MASS
DENSITY; QUIESCENT GALAXIES; FORMING GALAXIES; DISK GALAXIES;
SURFACE-DENSITY; FORMATION RATES; BULGE FORMATION; GALACTIC DISKS
AB It is well established that (1) star-forming galaxies follow a relation between their star formation rate (SFR) and stellar mass (M-*), the "star formation sequence," and (2) the SFRs of galaxies correlate with their structure, where star-forming galaxies are less concentrated than quiescent galaxies at fixed mass. Here, we consider whether the scatter and slope of the star formation sequence is correlated with systematic variations in the Sersic indices, n, of galaxies across the SFR-M-* plane. We use a mass-complete sample of 23,848 galaxies at 0.5 < z < 2.5 selected from the 3D-HST photometric catalogs. Galaxy light profiles parameterized by n are based on Hubble Space Telescope Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey near-infrared imaging. We use a single SFR indicator empirically calibrated from stacks of Spitzer/MIPS 24 mu m imaging, adding the unobscured and obscured star formation. We find that the scatter of the star formation sequence is related in part to galaxy structure; the scatter due to variations in n at fixed mass for star-forming galaxies ranges from 0.14 +/- 0.02 dex at z similar to 2 to 0.30 +/- 0.04 dex at z < 1. While the slope of the log SFR-log M-* relation is of order unity for disk-like galaxies, galaxies with n > 2 (implying more dominant bulges) have significantly lower SFR M-* than the main ridgeline of the star formation sequence. These results suggest that bulges in massive z similar to 2 galaxies are actively building up, where the stars in the central concentration are relatively young. At z < 1, the presence of older bulges within star-forming galaxies lowers global SFR M-*, decreasing the slope and contributing significantly to the scatter of the star formation sequence.
C1 [Whitaker, Katherine E.; Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Whitaker, Katherine E.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Franx, Marijn; Labbe, Ivo] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Bezanson, Rachel] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA.
[Brammer, Gabriel B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[van Dokkum, Pieter G.; Leja, Joel; Momcheva, Ivelina G.; Nelson, Erica J.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Kriek, Mariska T.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Rix, Hans-Walter; van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Skelton, Rosalind E.] S African Astron Observ, Observ, ZA-7935 Cape Town, South Africa.
[Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
RP Whitaker, KE (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
EM kwhitaker@astro.umass.edu
RI Skelton, Rosalind/S-1845-2016;
OI Skelton, Rosalind/0000-0001-7393-3336; Leja, Joel/0000-0001-6755-1315;
Bezanson, Rachel/0000-0001-5063-8254; Brammer,
Gabriel/0000-0003-2680-005X
FU NASA [NAS5-26555]; NASA through Hubble Fellowship - Space Telescope
Science Institute [HST-HF2-51368]; NASA/ESA HST [GO 12177, 12328]; NASA
Postdoctoral Program at the Goddard Space Flight Center
FX We thank the anonymous referee for a highly constructive report. This
work is based on observations taken by the 3D-HST Treasury Program (GO
12177 and 12328) with the NASA/ESA HST, which is operated by the
Associations of Universities for Resarch in Astronomy, Inc., under NASA
contract NAS5-26555. This research was supported in part by an
appointment to the NASA Postdoctoral Program at the Goddard Space Flight
Center, administered by Oak Ridge Associated Universities through a
contract with NASA and by NASA through Hubble Fellowship grant
HST-HF2-51368 awarded by the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., for NASA, under contract NAS5-26555.
NR 43
TC 18
Z9 18
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2015
VL 811
IS 1
AR L12
DI 10.1088/2041-8205/811/1/L12
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CV5VY
UT WOS:000364340600012
ER
PT J
AU Aartsen, MG
Abraham, K
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Ahrens, M
Altmann, D
Anderson, T
Archinger, M
Arguelles, C
Arlen, TC
Auffenberg, J
Bai, X
Barwick, SW
Baum, V
Bay, R
Beatty, JJ
Tjus, JB
Becker, KH
Beiser, E
BenZvi, S
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Bessonu, DZ
Binder, G
Bindig, D
Bissok, M
Blaueuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Borner, M
Bos, F
Bose, D
Boser, S
Botner, O
Braun, J
Brayeur, L
Bretz, HP
Brown, AM
Buzinsky, N
Casey, J
Casier, M
Cheung, E
Chirkin, D
Christov, A
Christy, B
Clark, K
Classen, L
Coenders, S
Cowen, DF
Silva, AHC
Daughhetee, J
Davis, JC
Day, M
de Andre, JPAM
De Clercq, C
Dembinski, H
De Ridder, S
Desiati, P
de Vries, KD
de Wasseige, G
de With, M
DeYoung, T
Diaz-Velez, JC
Dumm, JP
Dunkman, M
Eagan, R
Eberhardt, B
Ehrhardt, T
Eichmann, B
Euler, S
Evenson, PA
Fadiran, O
Fahey, S
Fazely, AR
Fedynitch, A
Feintzeig, J
Felde, J
Filimonov, K
Finley, C
Fischer-Wasels, T
Flis, S
Fuchs, T
Glagla, M
Gaisser, TK
Gator, R
Gallagher, J
Gerhardt, L
Ghorbani, K
Gier, D
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Golup, G
Gonzalez, JG
Gora, D
Grant, D
Gretskov, P
Groh, JC
Gross, A
Ha, C
Haack, C
Ismail, AH
Hallgren, A
Halzen, F
Hansmann, B
Hanson, K
Hebecker, D
Heereman, D
Helbing, K
Hellauer, R
Hellwig, D
Hickford, S
Hignight, J
Hill, GC
Hoffman, KD
Hoffmann, R
Holzapfe, K
Homeier, A
Hoshina, K
Huang, F
Huber, M
Huelsnitz, W
Hulth, PO
Hultqvist, K
In, S
Ishihara, A
Jacobi, E
Japaridze, GS
Jero, K
Jurkovic, M
Kaminsky, B
Kappes, A
Karg, T
Karle, A
Kauer, M
Keivani, A
Kelley, JL
Kemp, J
Kheirandish, A
Kiryluk, J
Klas, J
Klein, SR
Kohnen, G
Koirala, R
Kolanoski, H
Konietz, R
Koob, A
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krings, K
Kroll, G
Kroll, M
Kunnen, J
Kurahashi, N
Kuwabara, T
Labare, M
Lanfranchi, JL
Larson, MJ
Lesiak-Bzdak, M
Leuermann, M
Leuner, J
Lunemann, J
Madsen, J
Maggi, G
Mahn, KBM
Maruyama, R
Mase, K
Matis, HS
Maunu, R
McNally, F
Meagher, K
Medici, M
Meli, A
Menne, T
Merino, G
Meures, T
Miarecki, S
Middell, E
Middlemas, E
Miller, J
Mohrmann, L
Montaruli, T
Morse, R
Nahnhauer, R
Naumann, U
Niederhausen, H
Nowicki, SC
Nygre, DR
Obertacke, A
Olivas, A
Omairat, A
O'Murchadha, A
Palczewski, T
Pandya, H
Paul, L
Pepper, JA
de los Heros, CP
Pfendner, C
Pieloth, D
Pinat, E
Posselt, J
Price, PB
Przybylski, GT
Putz, J
Quinnan, M
Radel, L
Rameez, M
Rawlins, K
Redl, P
Reimann, R
Relich, M
Resconi, E
Rhode, W
Richman, M
Richter, S
Riedel, B
Robertson, S
Rongen, M
Rott, C
Ruhe, T
Ryckbosch, D
Saba, SM
Sabbatini, L
Sander, HG
Sandrock, A
Sandroos, J
Sarkar, S
Schatto, K
Scheriau, F
Schimp, M
Schmidt, T
Schmitz, M
Schoenen, S
Schoneberg, S
Schonwald, A
Schukraft, A
Schulte, L
Seckel, D
Seunarine, S
Shanidze, R
Smith, MWE
Soldin, D
Spiczak, GM
Ering, C
Stahlberg, M
Stamatikos, M
Stanev, T
Stanisha, NA
Stasik, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strahlers, EA
Strom, R
Strotjohann, NL
Suwvan, GW
Sutherland, M
Taavola, H
Taboada, I
Ter-Antonyan, S
Terliuk, A
Tesic, G
Tilav, S
Toale, PA
Tobin, MN
Tosi, D
Tselengidou, M
Turcati, A
Unger, E
Usner, M
Vallecorsa, S
van Eundhoven, N
Vandenbroucke, J
van Santen, J
Vanheule, S
Veenkamp, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Wallraff, M
Wandkowsky, N
Weaver, C
Wendt, C
Westerhoff, S
Whelan, BJ
Whitehorn, N
Wichary, C
Wiebe, K
Wiebusch, CH
Wille, L
Williams, DR
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, DL
Xu, XW
Xu, Y
Yanez, JP
Yodh, G
Yoshida, S
Zarzhitsky, P
Zoll, M
Ofek, EO
Kasliwal, MM
Nugent, PE
Arcavi, I
Bloom, JS
Kulkarni, SR
Perley, DA
Barlow, T
Horesh, A
Gal-Yam, A
Howell, DA
Dilday, B
Evans, PA
Kennea, JA
Burgett, WS
Chambers, KC
Kaiser, N
Waters, C
Flewelling, H
Tonry, JL
Rest, A
Smartt, SJ
AF Aartsen, M. G.
Abraham, K.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Ahrens, M.
Altmann, D.
Anderson, T.
Archinger, M.
Arguelles, C.
Arlen, T. C.
Auffenberg, J.
Bai, X.
Barwick, S. W.
Baum, V.
Bay, R.
Beatty, J. J.
Tjus, J. Becker
Becker, K. -H.
Beiser, E.
BenZvi, S.
Berghaus, P.
Berley, D.
Bernardini, E.
Bernhard, A.
Bessonu, D. Z.
Binder, G.
Bindig, D.
Bissok, M.
Blaueuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Boerner, M.
Bos, F.
Bose, D.
Boeser, S.
Botner, O.
Braun, J.
Brayeur, L.
Bretz, H. -P.
Brown, A. M.
Buzinsky, N.
Casey, J.
Casier, M.
Cheung, E.
Chirkin, D.
Christov, A.
Christy, B.
Clark, K.
Classen, L.
Coenders, S.
Cowen, D. F.
Silva, A. H. Cruz
Daughhetee, J.
Davis, J. C.
Day, M.
de Andre, J. P. A. M.
De Clercq, C.
Dembinski, H.
De Ridder, S.
Desiati, P.
de Vries, K. D.
de Wasseige, G.
de With, M.
DeYoung, T.
Diaz-Velez, J. C.
Dumm, J. P.
Dunkman, M.
Eagan, R.
Eberhardt, B.
Ehrhardt, T.
Eichmann, B.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fahey, S.
Fazely, A. R.
Fedynitch, A.
Feintzeig, J.
Felde, J.
Filimonov, K.
Finley, C.
Fischer-Wasels, T.
Flis, S.
Fuchs, T.
Glagla, M.
Gaisser, T. K.
Gator, R.
Gallagher, J.
Gerhardt, L.
Ghorbani, K.
Gier, D.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Gonzalez, J. G.
Gora, D.
Grant, D.
Gretskov, P.
Groh, J. C.
Gross, A.
Ha, C.
Haack, C.
Ismail, A. Haj
Hallgren, A.
Halzen, F.
Hansmann, B.
Hanson, K.
Hebecker, D.
Heereman, D.
Helbing, K.
Hellauer, R.
Hellwig, D.
Hickford, S.
Hignight, J.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Holzapfe, K.
Homeier, A.
Hoshina, K.
Huang, F.
Huber, M.
Huelsnitz, W.
Hulth, P. O.
Hultqvist, K.
In, S.
Ishihara, A.
Jacobi, E.
Japaridze, G. S.
Jero, K.
Jurkovic, M.
Kaminsky, B.
Kappes, A.
Karg, T.
Karle, A.
Kauer, M.
Keivani, A.
Kelley, J. L.
Kemp, J.
Kheirandish, A.
Kiryluk, J.
Klaes, J.
Klein, S. R.
Kohnen, G.
Koirala, R.
Kolanoski, H.
Konietz, R.
Koob, A.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Krings, K.
Kroll, G.
Kroll, M.
Kunnen, J.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Lanfranchi, J. L.
Larson, M. J.
Lesiak-Bzdak, M.
Leuermann, M.
Leuner, J.
Luenemann, J.
Madsen, J.
Maggi, G.
Mahn, K. B. M.
Maruyama, R.
Mase, K.
Matis, H. S.
Maunu, R.
McNally, F.
Meagher, K.
Medici, M.
Meli, A.
Menne, T.
Merino, G.
Meures, T.
Miarecki, S.
Middell, E.
Middlemas, E.
Miller, J.
Mohrmann, L.
Montaruli, T.
Morse, R.
Nahnhauer, R.
Naumann, U.
Niederhausen, H.
Nowicki, S. C.
Nygre, D. R.
Obertacke, A.
Olivas, A.
Omairat, A.
O'Murchadha, A.
Palczewski, T.
Pandya, H.
Paul, L.
Pepper, J. A.
de los Heros, C. Perez
Pfendner, C.
Pieloth, D.
Pinat, E.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Puetz, J.
Quinnan, M.
Raedel, L.
Rameez, M.
Rawlins, K.
Redl, P.
Reimann, R.
Relich, M.
Resconi, E.
Rhode, W.
Richman, M.
Richter, S.
Riedel, B.
Robertson, S.
Rongen, M.
Rott, C.
Ruhe, T.
Ryckbosch, D.
Saba, S. M.
Sabbatini, L.
Sander, H. -G.
Sandrock, A.
Sandroos, J.
Sarkar, S.
Schatto, K.
Scheriau, F.
Schimp, M.
Schmidt, T.
Schmitz, M.
Schoenen, S.
Schoeneberg, S.
Schoenwald, A.
Schukraft, A.
Schulte, L.
Seckel, D.
Seunarine, S.
Shanidze, R.
Smith, M. W. E.
Soldin, D.
Spiczak, G. M.
Ering, C.
Stahlberg, M.
Stamatikos, M.
Stanev, T.
Stanisha, N. A.
Stasik, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strahlers, E. A.
Strom, R.
Strotjohann, N. L.
Suwvan, G. W.
Sutherland, M.
Taavola, H.
Taboada, I.
Ter-Antonyan, S.
Terliuk, A.
Tesic, G.
Tilav, S.
Toale, P. A.
Tobin, M. N.
Tosi, D.
Tselengidou, M.
Turcati, A.
Unger, E.
Usner, M.
Vallecorsa, S.
van Eundhoven, N.
Vandenbroucke, J.
van Santen, J.
Vanheule, S.
Veenkamp, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Wallraff, M.
Wandkowsky, N.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whelan, B. J.
Whitehorn, N.
Wichary, C.
Wiebe, K.
Wiebusch, C. H.
Wille, L.
Williams, D. R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, D. L.
Xu, X. W.
Xu, Y.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
Zoll, M.
Ofek, Eran O.
Kasliwal, Mansi M.
Nugent, Peter E.
Arcavi, Iair
Bloom, Joshua S.
Kulkarni, Shrinivas R.
Perley, Daniel A.
Barlow, Tom
Horesh, Assaf
Gal-Yam, Avishay
Howell, D. A.
Dilday, Ben
Evans, Phil A.
Kennea, Jamie A.
Burgett, W. S.
Chambers, K. C.
Kaiser, N.
Waters, C.
Flewelling, H.
Tonry, J. L.
Rest, A.
Smartt, S. J.
CA IceCube Collaboration
PTF Collaboration
Swift Collaboration
Pan-STARRSi Sci Consortium
TI THE DETECTION OF A SN IIn IN OPTICAL FOLLOW-UP OBSERVATIONS OF ICECUBE
NEUTRINO EVENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; galaxies: dwarf; neutrinos; shock waves;
supernovae: individual (PTF12csy, SN 2010jl)
ID DIGITAL SKY SURVEY; HIGH-ENERGY NEUTRINOS; GAMMA-RAY BURSTS; EXTREMELY
LUMINOUS SUPERNOVA; CORE-COLLAPSE SUPERNOVAE; SDSS-III; LIGHT CURVES;
PAN-STARRS; TELESCOPE; EMISSION
AB The IceCube neutrino observatory pursues a follow-up program selecting interesting neutrino events in real-time and issuing alerts for electromagnetic follow-up observations. In 2012 March, the most significant neutrino alert during the first three years of operation was issued by IceCube. In the follow-up observations performed by the Palomar Transient Factory (PTF), a Type IIn supernova (SN IIn) PTF12csy was found 0.degrees 2 away from the neutrino alert direction, with an error radius of 0.degrees 54. It has a redshift of z = 0.0684, corresponding to a luminosity distance of about 300 Mpc and the Pan-STARRS1 survey shows that its explosion time was at least 158 days (in host galaxy rest frame) before the neutrino alert, so that a causal connection is unlikely. The a posteriori significance of the chance detection of both the neutrinos and the SN at any epoch is 2.2 sigma within IceCube's 2011/12 data acquisition season. Also, a complementary neutrino analysis reveals no long-term signal over the course of one year. Therefore, we consider the SN detection coincidental and the neutrinos uncorrelated to the SN. However, the SN is unusual and interesting by itself: it is luminous and energetic, bearing strong resemblance to the SN IIn 2010jl, and shows signs of interaction of the SN ejecta with a dense circumstellar medium. High-energy neutrino emission is expected in models of diffusive shock acceleration, but at a low, non-detectable level for this specific SN. In this paper, we describe the SN PTF12csy and present both the neutrino and electromagnetic data, as well as their analysis.
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[Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Kaminsky, B.; Karg, T.; Kowalski, M.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Ering, C.; Stasik, A.; Stoessl, A.; Strotjohann, N. L.; Terliuk, A.; Usner, M.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Adams, J.; Brown, A. M.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
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[Berley, D.; Blaueuss, E.; Cheung, E.; Christy, B.; Felde, J.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Maunu, R.; Olivas, A.; Redl, P.; Schmidt, T.; Suwvan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
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[Boersma, D. J.; Botner, O.; Euler, S.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.; Unger, E.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden.
[Boerner, M.; Fuchs, T.; Menne, T.; Pieloth, D.; Rhode, W.; Ruhe, T.; Sandrock, A.; Scheriau, F.; Schmitz, M.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Bose, D.; In, S.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
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[Buzinsky, N.; Grant, D.; Kopper, C.; Nowicki, S. C.; Riedel, B.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
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[Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[Clark, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Cowen, D. F.; Kennea, Jamie A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[de Andre, J. P. A. M.; DeYoung, T.; Hignight, J.; Mahn, K. B. M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
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[de With, M.; Hebecker, D.; Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, DeVment Phys, Baton Rouge, LA 70813 USA.
[Gator, R.; Ishihara, A.; Kuwabara, T.; Mase, K.; Relich, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Homeier, A.; Schulte, L.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Kauer, M.; Maruyama, R.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
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[Koskinen, D. J.; Larson, M. J.; Medici, M.; Sandroos, J.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
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[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
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[Kasliwal, Mansi M.] Carnegie Inst Sci, Pasadena, CA 91101 USA.
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[Dilday, Ben] North Idaho Coll, Coeur Dalene, ID 83814 USA.
[Evans, Phil A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
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RP Voge, M (reprint author), Univ Bonn, Inst Phys, Nussallee 12, D-53115 Bonn, Germany.
EM voge@physik.uni-bonn.de
RI Tjus, Julia/G-8145-2012; Maruyama, Reina/A-1064-2013; Beatty,
James/D-9310-2011; Horesh, Assaf/O-9873-2016; Wiebusch,
Christopher/G-6490-2012; Koskinen, David/G-3236-2014;
OI Arguelles Delgado, Carlos/0000-0003-4186-4182; Maruyama,
Reina/0000-0003-2794-512X; Beatty, James/0000-0003-0481-4952; Horesh,
Assaf/0000-0002-5936-1156; Wiebusch, Christopher/0000-0002-6418-3008;
Koskinen, David/0000-0002-0514-5917; Maunu, Ryan/0000-0002-5755-3437;
Perez de los Heros, Carlos/0000-0002-2084-5866; Sarkar,
Subir/0000-0002-3542-858X
FU U.S. National Science Foundation-Office of Polar Programs; U.S. National
Science Foundation-Physics Division; University of Wisconsin Alumni
Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid
infrastructure at the University of Wisconsin-Madison; Open Science Grid
(OSG) grid infrastructure; U.S. Department of Energy; National Energy
Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI); Natural Sciences and Engineering Research Council of
Canada; WestGrid; Compute/Calcul Canada; Swedish Research Council;
Swedish Polar Research Secretariat; Swedish National Infrastructure for
Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF); Deutsche
Forschungsgemeinschaft (DFG); Helmholtz Alliance for Astroparticle
Physics (HAP); Research Department of Plasmas with Complex Interactions
(Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus
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); W. M. Keck Foundation; Willner Family
Leadership Institute Ilan Gluzman (Secaucus NJ); Israeli Ministry of
Science; Israel Science Foundation; Minerva and the I-CORE Program of
the Planning and Budgeting Committee; UK Space Agency; UK Swift Science
Data Centre at the University of Leicester; National Aeronautics and
Space Administration [NNX08AR22G]; National Science Foundation
[AST-1238877]; ERC [291222]; Alfred P. Sloan Foundation; Participating
Institutions; National Science Foundation; U.S. Department of Energy
Office of Science
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).; This paper is based on
observations obtained with the Samuel Oschin Telescope as part of the
Palomar Transient Factory project, a scientific collaboration between
the California Institute of Technology, Columbia University, Las Cumbres
Observatory, the Lawrence Berkeley National Laboratory, the National
Energy Research Scientific Computing Center, the University of Oxford,
and the Weizmann Institute of Science. 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 are
grateful for excellent staff assistance at Palomar, Lick, and Keck
Observatories. E.O.O. is incumbent of the Arye Dissentshik career
development chair and is grateful to support by grants from the Willner
Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israeli Ministry
of Science, Israel Science Foundation, Minerva and the I-CORE Program of
the Planning and Budgeting Committee and The Israel Science Foundation.;
P. A. E. Acknowledges support from the UK Space Agency. This work made
use of data supplied by the UK Swift Science Data Centre at the
University of Leicester.; The Pan-STARRS1 Surveys (PS1) have been made
possible through contributions of the Institute for Astronomy, the
University of Hawaii, the Pan-STARRS Project Office, the Max-Planck
Society and its participating institutes, the Max Planck Institute for
Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial
Physics, Garching, The Johns Hopkins University, Durham University, the
University of Edinburgh, Queen's University Belfast, the
Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory
Global Telescope Network Incorporated, the National Central University
of Taiwan, the Space Telescope Science Institute, the National
Aeronautics and Space Administration under Grant No. NNX08AR22G issued
through the Planetary Science Division of the NASA Science Mission
Directorate, the National Science Foundation under Grant No.
AST-1238877, the University of Maryland, and Eotvos Lorand University
(ELTE).; S.J.S. acknowledges (FP7/2007-2013)/ERC grant agreement no
[291222].; 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/.
NR 89
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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 SEP 20
PY 2015
VL 811
IS 1
AR 52
DI 10.1088/0004-637X/811/1/52
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU4BR
UT WOS:000363471600053
ER
PT J
AU Caliandro, GA
Cheung, CC
Li, J
Scargle, JL
Torres, DF
Wood, KS
Chernyakova, M
AF Caliandro, G. A.
Cheung, C. C.
Li, J.
Scargle, J. L.
Torres, D. F.
Wood, K. S.
Chernyakova, M.
TI GAMMA-RAY FLARE ACTIVITY FROM PSR B1259-63 DURING 2014 PERIASTRON
PASSAGE AND COMPARISON TO ITS 2010 PASSAGE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: stars; pulsars: individual (PSR B1259-63); X-rays: binaries
ID BINARY-SYSTEM; PULSAR WIND; TELESCOPE; AREA; PSR-1259-63; EMISSION;
CATALOG; RADIO
AB PSR B1259-63/LS 2883 is a gamma-ray binary system containing a radio pulsar in a highly elliptical similar to 3.4-year orbit around a Be star. In its 2010 periastron passage, multiwavelength emission from radio to TeV was observed, as well as an unexpected GeV flare measured by the Fermi Large Area Telescope (LAT). Here, we report the results of LAT monitoring of PSR B1259-63 during its most recent 2014 periastron passage. We compare the gamma-ray behavior in this periastron with the former in 2010 and find that PSR B1259-63 shows a recurrent GeV flare. The similarities and differences in the phenomenology of both periastron passages are discussed.
C1 [Caliandro, G. A.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Caliandro, G. A.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Caliandro, G. A.] CIFS, Laquila, Italy.
[Cheung, C. C.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Li, J.; Torres, D. F.] Inst Space Sci CSIC IEEC, E-08193 Barcelona, Spain.
[Scargle, J. L.] NASA Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Torres, D. F.] ICREA, E-08010 Barcelona, Spain.
[Chernyakova, M.] Dublin City Univ, Dublin 9, Ireland.
[Chernyakova, M.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland.
RP Caliandro, GA (reprint author), Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM caliandr@slac.stanford.edu; jian@ieec.uab.es; kent.wood@nrl.navy.mil
RI Torres, Diego/O-9422-2016
OI Torres, Diego/0000-0002-1522-9065
FU Commonwealth Government; National Natural Science Foundation of China
[AYA2012-39303, SGR 2014-1073, NSFC-11473027]; Chinese Academy of
Sciences visiting professorship program [2013T2J0007]; NASA [DPR
S-15633-Y]
FX The Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), the High
Energy Accelerator Research Organization (KEK), and the Japan Aerospace
Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation,
the Swedish Research Council, and the Swedish National Space Board in
Sweden. Additional support for science analysis during the operations
phase is gratefully acknowledged from the Istituto Nazionale di
Astrofisica in Italy and the Centre National d'Etudes Spatiales in
France. The Parkes radio telescope is part of the Australia Telescope,
which is funded by the Commonwealth Government for operation as a
National Facility managed by CSIRO. We thank our colleagues for their
assistance with the radio timing observations. J.L. and D.F.T.
acknowledge support from the grants AYA2012-39303 and SGR 2014-1073, and
support from the National Natural Science Foundation of China via
NSFC-11473027. D.F.T. further acknowledges the Chinese Academy of
Sciences visiting professorship program 2013T2J0007. Work by C.C.C at
the NRL is supported in part by NASA DPR S-15633-Y.
NR 28
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
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VL 811
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AR 68
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PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU4BR
UT WOS:000363471600069
ER
PT J
AU Harding, AK
Kalapotharakos, C
AF Harding, Alice K.
Kalapotharakos, Constantinos
TI SYNCHROTRON SELF-COMPTON EMISSION FROM THE CRAB AND OTHER PULSARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: stars; pulsars: general; radiation mechanisms: non-thermal;
relativistic processes; stars: neutron; X-rays: stars
ID HIGH-ENERGY EMISSION; GAMMA-RAY PULSARS; LARGE-AREA TELESCOPE;
MILLISECOND PULSAR; RADIO-EMISSION; OUTER MAGNETOSPHERE;
MAGNETIC-FIELDS; PAIR PRODUCTION; LIGHT CURVES; LOW-ALTITUDE
AB Results of a simulation of synchrotron self-Compton (SSC) emission from a rotation-powered pulsar are presented. The radiating particles are assumed to be both accelerated primary electrons and a spectrum of electron-positron pairs produced in cascades near the polar cap. They follow trajectories in a slot gap using 3D force-free magnetic field geometry, gaining pitch angles through resonant cyclotron absorption of radio photons, radiating and scattering synchrotron emission at high altitudes out to and beyond the light cylinder. Full angular dependence of the synchrotron photon density is simulated in the scattering and all processes are treated in the inertial observer frame. Spectra for the Crab and Vela pulsars as well as two energetic millisecond pulsars, B1821-24 and B1937+21, are simulated using this model. The simulation of the Crab pulsar radiation can reproduce both the flux level and the shape of the observed optical to hard X-ray emission assuming a pair multiplicity of M+ = 3 x 10(5), as well as the very-high-energy emission above 50 GeV detected by MAGIC and VERITAS, with both the synchrotron and SSC components reflecting the shape of the pair spectrum. Simulations of Vela, B1821-24, and B1937+21, for M+ up to 105, do not produce pair SSC emission that is detectable by current telescopes, indicating that only Crab-like pulsars produce significant SSC components. The pair synchrotron emission matches the observed X-ray spectrum of the millisecond pulsars, and the predicted peak of this emission at 1-10 MeV would be detectable with planned Compton telescopes.
C1 [Harding, Alice K.; Kalapotharakos, Constantinos] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Kalapotharakos, Constantinos] Univ Maryland, Coll Pk UMDCP CRESST, College Pk, MD 20742 USA.
RP Harding, AK (reprint author), NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
FU NASA Astrophysics Theory Program; Fermi Guest Investigator Program; NASA
High-end Computing (HEC) Program through the NASA Center for Climate
Simulation (NCCS) at Goddard Space Flight Center
FX We would like to thank Isabelle Grenier, Andrey Timokhin, and Christo
Venter for helpful discussions and acknowledge support from the NASA
Astrophysics Theory Program and the Fermi Guest Investigator Program.
Resources supporting this work were provided by the NASA High-end
Computing (HEC) Program through the NASA Center for Climate Simulation
(NCCS) at Goddard Space Flight Center. We thank Craig Pelissier of the
NCCS in particular for help with parallel processing.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
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JI Astrophys. J.
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PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU4BR
UT WOS:000363471600064
ER
PT J
AU Hippke, M
Angerhausen, D
AF Hippke, Michael
Angerhausen, Daniel
TI A STATISTICAL SEARCH FOR A POPULATION OF EXO-TROJANS IN THE KEPLER DATA
SET
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids: general; planets and satellites: general
AB Trojans are small bodies in planetary Lagrangian points. In our solar system, Jupiter has the largest number of such companions. Their existence is assumed for exoplanetary systems as well, but none have been found so far. We present an analysis by super-stacking similar to 4 x 10(3) Kepler planets with a total of similar to 9 x 10(4) transits, searching for an average Trojan transit dip. Our results give an upper limit to the average Trojan transiting area (per planet) that corresponds to one body of radius <460 km with 2 sigma confidence. We find a significant Trojan-like signal in a subsample for planets with more (or larger) Trojans for periods >60 days. Our tentative results can and should be checked with improved data from future missions like PLATO 2.0, and can guide planetary formation theories.
C1 [Angerhausen, Daniel] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hippke, M (reprint author), Luiter Str 21b, D-47506 Neukirchen Vluyn, Germany.
EM hippke@ifda.eu; daniel.angerhausen@nasa.gov
NR 31
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2015
VL 811
IS 1
AR 1
DI 10.1088/0004-637X/811/1/1
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU4BR
UT WOS:000363471600001
ER
PT J
AU Lalitha, S
Singh, KP
Drake, SA
Kashyap, V
AF Lalitha, S.
Singh, K. P.
Drake, S. A.
Kashyap, V.
TI X-RAYING THE CORONAE OF HD 155555
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: activity; stars: coronae; stars: individual (HD 155555); stars:
low-mass; stars: pre-main sequence; techniques: spectroscopic
ID T-TAURI STARS; MAIN-SEQUENCE BINARY; HELIUM-LIKE IONS; EMISSION MEASURE
DISTRIBUTIONS; RS-CVN; XMM-NEWTON; AR LACERTAE; SPECTRAL VARIABILITY;
EVOLUTIONARY STATUS; LIGHT MEASUREMENTS
AB We present an analysis of the high-resolution Chandra observation of the multiple system, HD 155555 (an RS Canum Venaticorum; RS CVn type binary system, HD 155555 AB, and its spatially resolved low-mass companion HD 155555 C). This is an intriguing system that shows properties of both an active pre-main-sequence star and a synchronized (main sequence) binary. We obtain the emission measure distribution, temperature structures, plasma densities, and abundances of this system and compare them with the coronal properties of other young/active stars. HD 155555 AB and HD 155555 C produce copious X-ray emission with log L-x of 30.54 and 29.30, respectively, in the 0.3-6.0 keV energy band. The light curves of individual stars show variability on timescales of a few minutes to hours. We analyze the dispersed spectra and reconstruct the emission measure distribution using spectral line analysis. The resulting elemental abundances exhibit an inverse first ionization potential effect in both cases. An analysis of He-like triplets yields a range of coronal electron densities similar to 10(10) - 10(13) cm(-3). Since HD 155555 AB is classified as both an RS CVn and a PMS star, we compare our results with those of other slightly older active main-sequence stars and T Tauri stars, which indicate that the coronal properties of HD 155555 AB closely resemble that of an older RS CVn binary rather than a younger PMS star. Our results also suggest that the properties of HD 155555 C are very similar to those of other active M dwarfs.
C1 [Lalitha, S.; Singh, K. P.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Drake, S. A.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kashyap, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Lalitha, S (reprint author), Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India.
NR 83
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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 SEP 20
PY 2015
VL 811
IS 1
AR 44
DI 10.1088/0004-637X/811/1/44
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU4BR
UT WOS:000363471600045
ER
PT J
AU Millar-Blanchaer, MA
Graham, JR
Pueyo, L
Kalas, P
Dawson, RI
Wang, J
Perrin, MD
Moon, DS
Macintosh, B
Ammons, SM
Barman, T
Cardwell, A
Chen, CH
Chiang, E
Chilcote, J
Cotten, T
De Rosa, RJ
Draper, ZH
Dunn, J
Duchene, G
Esposito, TM
Fitzgerald, MP
Follette, KB
Goodsell, SJ
Greenbaum, AZ
Hartung, M
Hibon, P
Hinkley, S
Ingraham, P
Jensen-Clem, R
Konopacky, Q
Larkin, JE
Long, D
Maire, J
Marchis, F
Marley, MS
Marois, C
Morzinski, KM
Nielsen, EL
Palmer, DW
Oppenheimer, R
Poyneer, L
Rajan, A
Rantakyro, FT
Ruffio, JB
Sadakuni, N
Saddlemyer, L
Schneider, AC
Sivaramakrishnan, A
Soummer, R
Thomas, S
Vasisht, G
Vega, D
Wallace, JK
Ward-Duong, K
Wiktorowicz, SJ
Wolff, SG
AF Millar-Blanchaer, Maxwell A.
Graham, James R.
Pueyo, Laurent
Kalas, Paul
Dawson, Rebekah I.
Wang, Jason
Perrin, Marshall D.
Moon, Dae-Sik
Macintosh, Bruce
Ammons, S. Mark
Barman, Travis
Cardwell, Andrew
Chen, Christine H.
Chiang, Eugene
Chilcote, Jeffrey
Cotten, Tara
De Rosa, Robert J.
Draper, Zachary H.
Dunn, Jennifer
Duchene, Gaspard
Esposito, Thomas M.
Fitzgerald, Michael P.
Follette, Katherine B.
Goodsell, Stephen J.
Greenbaum, Alexandra Z.
Hartung, Markus
Hibon, Pascale
Hinkley, Sasha
Ingraham, Patrick
Jensen-Clem, Rebecca
Konopacky, Quinn
Larkin, James E.
Long, Douglas
Maire, Jerome
Marchis, Franck
Marley, Mark S.
Marois, Christian
Morzinski, Katie M.
Nielsen, Eric L.
Palmer, David W.
Oppenheimer, Rebecca
Poyneer, Lisa
Rajan, Abhijith
Rantakyroe, Fredrik T.
Ruffio, Jean-Baptiste
Sadakuni, Naru
Saddlemyer, Leslie
Schneider, Adam C.
Sivaramakrishnan, Anand
Soummer, Remi
Thomas, Sandrine
Vasisht, Gautam
Vega, David
Wallace, J. Kent
Ward-Duong, Kimberly
Wiktorowicz, Sloane J.
Wolff, Schuyler G.
TI beta PICTORIS' INNER DISK IN POLARIZED LIGHT AND NEW ORBITAL PARAMETERS
FOR beta PICTORIS b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrometry; planet-disk interactions; planets and satellites: individual
(beta Pic b); techniques: polarimetric
ID GEMINI PLANET IMAGER; DEBRIS DISK; IMAGING POLARIMETRY; CIRCUMSTELLAR
DISK; GIANT PLANET; MOVING GROUP; 1ST LIGHT; DUST DISK; SYSTEM; BODIES
AB We present H-band observations of beta Pic with the Gemini Planet Imager's (GPI's) polarimetry mode that reveal the debris disk between similar to 0 ''.3 (6AU) and similar to 1 ''.7 (33 AU), while simultaneously detecting beta Pic b. The polarized disk image was fit with a dust density model combined with a Henyey-Greenstein scattering phase function. The best-fit model indicates a disk inclined to the line of sight (phi = 85 degrees.27(-0.19)(+0.26)) with a position angle (PA) theta(PA) = 30 degrees.35(-0.28)(+0.29) (slightly offset from the main outer disk, theta(PA) approximate to 29 degrees), that extends from an inner disk radius of 23.6(-0.6)(+0.9) AU to well outside GPI's field of view. In addition, we present an updated orbit for beta Pic b based on new astrometric measurements taken in GPI's spectroscopic mode spanning 14 months. The planet has a semimajor axis of a = 9.2(-0.4)(+1.5) AU, with an eccentricity e <= 0.26. The PA of the ascending node is Omega = 31 degrees.75 +/- 0 degrees.15, offset from both the outer main disk and the inner disk seen in the GPI image. The orbital fit constrains the stellar mass of beta Pic to 1.60 +/- 0.05 M-circle dot. Dynamical sculpting by beta Pic b cannot easily account for the following three aspects of the inferred disk properties: (1) the modeled inner radius of the disk is farther out than expected if caused by beta Pic b; (2) the mutual inclination of the inner disk and beta Pic b is similar to 4 degrees, when it is expected to be closer to zero; and (3) the aspect ratio of the disk (h(0) = 0.137(-0.006)(+0.005)) is larger than expected from interactions with beta Pic b or self-stirring by the disk's parent bodies.
C1 [Millar-Blanchaer, Maxwell A.; Moon, Dae-Sik] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M55 3H4, Canada.
[Graham, James R.; Kalas, Paul; Dawson, Rebekah I.; Wang, Jason; Chiang, Eugene; De Rosa, Robert J.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Perrin, Marshall D.; Chen, Christine H.; Long, Douglas; Sivaramakrishnan, Anand; Soummer, Remi] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Macintosh, Bruce; Follette, Katherine B.; Nielsen, Eric L.; Ruffio, Jean-Baptiste] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Ammons, S. Mark; Palmer, David W.; Poyneer, Lisa] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA.
[Barman, Travis] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Cardwell, Andrew; Hartung, Markus; Hibon, Pascale; Rantakyroe, Fredrik T.] Gemini Observ, La Serena, Chile.
[Chilcote, Jeffrey; Maire, Jerome] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M55 3H4, Canada.
[Cotten, Tara] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
[Draper, Zachary H.] Univ Victoria, Victoria, BC V8P 5C2, Canada.
[Draper, Zachary H.; Dunn, Jennifer; Marois, Christian; Saddlemyer, Leslie] Natl Res Council Canada Herzberg, Victoria, BC V9E 2E7, Canada.
[Duchene, Gaspard] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France.
[Esposito, Thomas M.; Fitzgerald, Michael P.; Larkin, James E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Goodsell, Stephen J.] Gemini Observ, Hilo, HI 96720 USA.
[Greenbaum, Alexandra Z.; Wolff, Schuyler G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hinkley, Sasha] Univ Exeter, Coll Engn Math & Phys Sci, Sch Phys, Exeter EX4 4QL, Devon, England.
[Ingraham, Patrick; Thomas, Sandrine] Large Synopt Survey Telescope, Tucson, AZ 85719 USA.
[Jensen-Clem, Rebecca] CALTECH, Dept Astrophys, Pasadena, CA 91101 USA.
[Konopacky, Quinn] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Marchis, Franck; Nielsen, Eric L.; Vega, David] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
[Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Morzinski, Katie M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Pueyo, Laurent; Oppenheimer, Rebecca] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
[Rajan, Abhijith; Ward-Duong, Kimberly] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Sadakuni, Naru] Univ Space Res Assoc, Stratospher Observ Infrared Astron, NASA, Armstrong Flight Res Ctr, Palmdale, CA 93550 USA.
[Schneider, Adam C.] Univ Toledo, Toledo, OH 43606 USA.
[Vasisht, Gautam; Wallace, J. Kent] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Vega, David] Calif State Polytech Univ Pomona, Dept Phys & Astron, Pomona, CA 91768 USA.
[Wiktorowicz, Sloane J.] UC Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
RP Millar-Blanchaer, MA (reprint author), Univ Toronto, Dept Astron & Astrophys, Toronto, ON M55 3H4, Canada.
EM maxmb@astro.utoronto.ca
OI Oppenheimer, Rebecca/0000-0001-7130-7681; Marley,
Mark/0000-0002-5251-2943; Morzinski, Katie/0000-0002-1384-0063; Wang,
Jason/0000-0003-0774-6502; Greenbaum, Alexandra/0000-0002-7162-8036
FU NASA [NNX15AD95G, NASA NNX11AD21G, NSF AST-0909188]; University of
California [LFRP-118057]; UC Berkeley Miller Institute for Basic
Research; NASA ATP program; U.S. Department of Energy by Lawrence
Livermore National Laboratory [DE-AC52-07NA27344]; NSF [AST1-413718,
DGE-1232825]; NASA
FX The results presented herein are based on observations carried out
during the commissioning of GPI as well as observations from the general
observing program GS-2014B-Q-48. The Gemini Observatory is operated by
the Association of Universities for Research in Astronomy, Inc., under a
cooperative agreement with the NSF on behalf of the Gemini partnership:
the National Science Foundation (United States), the 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 was supported in part by NASA cooperative agreement
NNX15AD95G, NASA NNX11AD21G, NSF AST-0909188, and the University of
California LFRP-118057. R.I.D gratefully acknowledges funding by the UC
Berkeley Miller Institute for Basic Research. M.S.M. acknowledges the
support of the NASA ATP program. S.M.A.'s work was performed under the
auspices of the U.S. Department of Energy by Lawrence Livermore National
Laboratory under Contract DE-AC52-07NA27344. M.P.F.'s and G.D.'s work
was carried out with contributions from NSF grant AST1-413718. S.
Wiktorowicz's work was performed (in part) under contract with the
California Institute of Technology (Caltech) funded by NASA through the
Sagan Fellowship Program executed by the NASA Exoplanet Science
Institute. The work of A. G. is supported by the NSF Graduate Research
Fellowship Program under grant No. DGE-1232825. Portions of D.W.P.'s
work were performed under the auspices of the U.S. Department of Energy
by Lawrence Livermore National Laboratory under Contract
DE-AC52-07NA27344. All posterior distribution plots have been created
with the Triangle33 python plotting package (Foreman-Mackey et al.
2014).
NR 78
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Z9 26
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2015
VL 811
IS 1
AR 18
DI 10.1088/0004-637X/811/1/18
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU4BR
UT WOS:000363471600019
ER
PT J
AU Miller, AA
AF Miller, A. A.
TI THE SYNTHETIC-OVERSAMPLING METHOD: USING PHOTOMETRIC COLORS TO DISCOVER
EXTREMELY METAL-POOR STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; methods: statistical; stars: general; stars:
statistics; stars: fundamental parameters; surveys
ID DIGITAL SKY SURVEY; HIGH-RESOLUTION SPECTROSCOPY; I. ATMOSPHERIC
PARAMETERS; MILKY-WAY TOMOGRAPHY; STELLAR METALLICITY; SDSS-III;
HAMBURG/ESO SURVEY; VARIABLE-STARS; DATA RELEASE; STRIPE 82
AB Extremely metal-poor (EMP) stars ([Fe/H] <= -3.0 dex) provide a unique window into understanding the first generation of stars and early chemical enrichment of the universe. EMP stars are exceptionally rare, however, and the relatively small number of confirmed discoveries limits our ability to exploit these near-field probes of the first similar to 500 Myr after the Big Bang. Here, a new method to photometrically estimate [Fe/H] from only broadband photometric colors is presented. I show that the method, which utilizes machine-learning algorithms and a training set of similar to 170,000 stars with spectroscopically measured [Fe/H], produces a typical scatter of similar to 0.29 dex. This performance is similar to what is achievable via low-resolution spectroscopy, and outperforms other photometric techniques, while also being more general. I further show that a slight alteration to the model, wherein synthetic EMP stars are added to the training set, yields the robust identification of EMP candidates. In particular, this synthetic-oversampling method recovers similar to 20% of the EMP stars in the training set, at a precision of similar to 0.05. Furthermore, similar to 65% of the false positives from the model are very metal-poor stars ([Fe/H] <= -2.0 dex). The synthetic-oversampling method is biased toward the discovery of warm (similar to F-type) stars, a consequence of the targeting bias from the Sloan Digital Sky Survey/Sloan Extension for Galactic Understanding survey. This EMP selection method represents a significant improvement over alternative broadband optical selection techniques. The models are applied to >12 million stars, with an expected yield of similar to 600 new EMP stars, which promises to open new avenues for exploring the early universe.
C1 [Miller, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Miller, A. A.] CALTECH, Pasadena, CA 91125 USA.
RP Miller, AA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-506, Pasadena, CA 91109 USA.
EM amiller@astro.caltech.edu
FU NASA from a Hubble Fellowship [HST-HF-51325.01]; STScI; NASA [NAS
5-26555]; Alfred P. Sloan Foundation; National Science Foundation; U. S.
Department of Energy Office of Science; University of Arizona; Brazilian
Participation Group; Brookhaven National Laboratory; Carnegie Mellon
University; University of Florida; French Participation Group; German
Participation Group, Harvard University; Instituto de Astrofisica de
Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns
Hopkins University; Lawrence Berkeley National Laboratory; Max Planck
Institute for Astrophysics; Max Planck Institute for Extraterrestrial
Physics, New Mexico State University, New York University; Ohio State
University; Pennsylvania State University; University of Portsmouth;
Princeton University; Spanish Participation Group; University of Tokyo;
University of Utah; Vanderbilt University; University of Virginia;
University of Washington; Yale University
FX I thank B. Bue and U. Rebbapragada for multiple useful conversations on
class imbalance and model optimization. I am grateful that J. Cohen was
willing to suffer many (possibly naive) questions about stellar
metallicity measurements and bias in the SDSS sample. J. Cohen, L.
Hillenbrand, and E. Kirby provided comments on an early version of this
paper, which greatly improved its final content. An anonymous referee
provided multiple suggestions that improved the discussion presented
herein. Finally, I thank the SEGUE team for making the results of the
SSPP public, and I am especially indebted to Y. S. Lee, who has answered
many inquiries about the SSPP flags and the reliability of the
individual [Fe/H] measurement methods. I acknowledge support for this
work by NASA from a Hubble Fellowship grant: HST-HF-51325.01, awarded by
STScI, operated by AURA, Inc., for NASA, under contract NAS 5-26555.
Part of the research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. 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.
NR 65
TC 1
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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 SEP 20
PY 2015
VL 811
IS 1
AR 30
DI 10.1088/0004-637X/811/1/30
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU4BR
UT WOS:000363471600031
ER
PT J
AU Panesar, NK
Sterling, AC
Innes, DE
Moore, RL
AF Panesar, Navdeep K.
Sterling, Alphonse C.
Innes, Davina E.
Moore, Ronald L.
TI DESTABILIZATION OF A SOLAR PROMINENCE/FILAMENT FIELD SYSTEM BY A SERIES
OF EIGHT HOMOLOGOUS ERUPTIVE FLARES LEADING TO A CME
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: coronal mass ejections (CMEs); Sun: filaments; prominences; Sun:
flares
ID CORONAL MASS EJECTIONS; 1973 JANUARY 11; 9 R PERIOD; EMERGING FLUX;
FILAMENT-ERUPTION; MAGNETIC-FIELDS; ONSET; DYNAMICS; CAVITY; EVENT
AB Homologous flares are flares that occur repetitively in the same active region, with similar structure and morphology. A series of at least eight homologous flares occurred in active region NOAA 11237 over 2011 June 16-17. A nearby prominence/filament was rooted in the active region, and situated near the bottom of a coronal cavity. The active region was on the southeast solar limb as seen from the Solar Dynamics Observatory/Atmospheric Imaging Assembly, and on the disk as viewed from the Solar TErrestrial RElations Observatory/EUVI-B. The dual perspective allows us to study in detail behavior of the prominence/filament material entrained in the magnetic field of the repeatedly erupting system. Each of the eruptions were mainly confined, but expelled hot material into the prominence/filament cavity system (PFCS). The field carrying and containing the ejected hot material interacted with the PFCS and caused it to inflate, resulting in a step-wise rise of the PFCS approximately in step with the homologous eruptions. The eighth eruption triggered the PFCS to move outward slowly, accompanied by a weak coronal dimming. As this slow PFCS eruption was underway, a final "ejective" flare occurred in the core of the active region, resulting in strong dimming in the EUVI-B images and expulsion of a coronal mass ejection (CME). A plausible scenario is that the repeated homologous flares could have gradually destabilized the PFCS, and its subsequent eruption removed field above the acitive region and in turn led to the ejective flare, strong dimming, and CME.
C1 [Panesar, Navdeep K.; Moore, Ronald L.] UAH, CSPAR, Huntsville, AL 35805 USA.
[Sterling, Alphonse C.; Moore, Ronald L.] NASA, George C Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, Huntsville, AL 35812 USA.
[Innes, Davina E.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
RP Panesar, NK (reprint author), UAH, CSPAR, Huntsville, AL 35805 USA.
EM navdeep.k.panesar@nasa.gov
OI Panesar, Navdeep/0000-0001-7620-362X
FU Heliophysics Division of NASA's Science Mission Directorate through the
Living With a Star Targeted Research and Technology Program; Hinode
Project
FX We acknowledge the use of the SDO/AIA, STEREO/EUVI observations for this
study. SDO data are courtesy of the NASA/SDO AIA and HMI science teams.
STEREO data are courtesy of the STEREO Sun Earth Connection Coronal and
Heliospheric Investigation (SECCHI) team. This work was supported by the
Heliophysics Division of NASA's Science Mission Directorate through the
Living With a Star Targeted Research and Technology Program, and by the
Hinode Project.
NR 61
TC 1
Z9 1
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 SEP 20
PY 2015
VL 811
IS 1
AR 5
DI 10.1088/0004-637X/811/1/5
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU4BR
UT WOS:000363471600005
ER
PT J
AU Rudy, A
Horns, D
DeLuca, A
Kolodziejczak, J
Tennant, A
Yuan, YJ
Buehler, R
Arons, J
Blandford, R
Caraveo, P
Costa, E
Funk, S
Hays, E
Lobanov, A
Max, C
Mayer, M
Mignani, R
O'Dell, SL
Romani, R
Tavani, M
Weisskopf, MC
AF Rudy, Alexander
Horns, Dieter
DeLuca, Andrea
Kolodziejczak, Jeffery
Tennant, Allyn
Yuan, Yajie
Buehler, Rolf
Arons, Jonathon
Blandford, Roger
Caraveo, Patrizia
Costa, Enrico
Funk, Stephan
Hays, Elizabeth
Lobanov, Andrei
Max, Claire
Mayer, Michael
Mignani, Roberto
O'Dell, Stephen L.
Romani, Roger
Tavani, Marco
Weisskopf, Martin C.
TI CHARACTERIZATION OF THE INNER KNOT OF THE CRAB: THE SITE OF THE
GAMMA-RAY FLARES?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: jets and outflows; ISM: supernova remnants; pulsars: individual
(Crab); techniques: image processing
ID PULSAR WIND NEBULAE; PARTICLE-ACCELERATION; MAGNETOHYDRODYNAMIC
SIMULATIONS; MAGNETIC RECONNECTION; OBLIQUE ROTATORS; 2011 APRIL;
EMISSION; ORIGIN; VARIABILITY; DISCOVERY
AB A particularly intriguing recent result from gamma-ray astronomy missions is the detection of powerful flares from the Crab Nebula, which challenges the current understanding of pulsar wind nebulae and acceleration mechanisms. To search for the production site(s) of these flares, we conducted a multi-wavelength observing campaign using Keck, the Hubble Space Telescope (HST), and the Chandra X-ray Observatory. As the short timescales of the gamma-ray flares (less than or similar to 1 day) suggest a small emitting region, the Crab's inner knot (about 0.6 arcsec from the pulsar) is a candidate site for such flaring. This paper describes observations of the inner knot, seeking to understand its nature and possible relationship with gamma-ray flares. Using singular-value decomposition, analysis of the HST images yielded results consistent with traditional methods while substantially reducing some uncertainties. These analyses show that the knot's intrinsic properties (especially size and brightness) are correlated with its (projected) separation from the pulsar. This characterization of the inner knot helps in constraining standard shock model parameters, under the assumption that the knot lies near the shocked surface. While the standard shock model gives good agreement in several respects, two puzzles persist: (a) the observed angular size of the knot relative to the pulsar-knot separation is much smaller than expected; and (b) the variable high degree of polarization (reported by others) is difficult to reconcile with a highly relativistic downstream flow. However, the IR-optical flux of the inner knot is marginally consistent with the shock accelerating most of the Nebula's optical-emitting particles.
C1 [Rudy, Alexander; Tavani, Marco] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Horns, Dieter] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany.
[DeLuca, Andrea; Caraveo, Patrizia; Mignani, Roberto; Tavani, Marco] INAF IASF Milano, I-20133 Milan, Italy.
[DeLuca, Andrea; Caraveo, Patrizia; Tavani, Marco] Ist Nazl Fis Nucl, I-27100 Pavia, Italy.
[Kolodziejczak, Jeffery; Tennant, Allyn; O'Dell, Stephen L.; Weisskopf, Martin C.] NASA, George C Marshall Space Flight Ctr, Astrophys Off ZP12, Huntsville, AL 35812 USA.
[Yuan, Yajie; Blandford, Roger; Funk, Stephan; Romani, Roger] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Buehler, Rolf; Mayer, Michael] DESY, D-15738 Zeuthen, Germany.
[Arons, Jonathon] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Arons, Jonathon] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA.
[Costa, Enrico] INFN Roma Tor Vergata, I-00133 Rome, Italy.
[Hays, Elizabeth] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Lobanov, Andrei] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Mignani, Roberto] Univ Zielona Gora, Kepler Inst Astron, PL-65265 Zielona Gora, Poland.
RP Rudy, A (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
RI Funk, Stefan/B-7629-2015;
OI Funk, Stefan/0000-0002-2012-0080; Tavani, Marco/0000-0003-2893-1459;
O'Dell, Stephen/0000-0002-1868-8056; Costa, Enrico/0000-0003-4925-8523
FU National Aeronautics and Space Administration; Department of Energy in
the United States; Commissariat a l'Energie Atomique; Centre National de
la Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France; Agenzia Spaziale Italiana; Istituto
Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture,
Sports, Science, and Technology (MEXT); High Energy Accelerator Research
Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan;
K. A. Wallenberg Foundation; Swedish Research Council; Swedish National
Space Board in Sweden; Istituto Nazionale di Astrofisica; Centre
d'Etudes Spatiales in France; European Commission Seventh Framework
Programme (FP7) [267251]; Chandra X-ray Center; Hubble Space Telescope
Science Institute [GO3-14054Z, GO3-14057Z, GO4-15058Z, GO4-15059Z,
GO-13109, GO-13196, GO-13348]
FX The Fermi/LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science, and Technology (MEXT), High Energy
Accelerator Research Organization (KEK), and the Japan Aerospace
Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation,
the Swedish Research Council, and the Swedish National Space Board in
Sweden. Additional support for science analysis during the operations
phase is gratefully acknowledged from the Istituto Nazionale di
Astrofisica and the Centre d'Etudes Spatiales in France. The research
leading to these results has also received funding from the European
Commission Seventh Framework Programme (FP7/2007-2013) under grant
agreement n. 267251. Several of the authors would also like to
acknowledge both funding and solid support from the Chandra X-ray Center
and the Hubble Space Telescope Science Institute under a number of
observing proposals: GO3-14054Z, GO3-14057Z, GO4-15058Z, GO4-15059Z,
GO-13109, GO-13196, and GO-13348.
NR 49
TC 8
Z9 8
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 SEP 20
PY 2015
VL 811
IS 1
AR 24
DI 10.1088/0004-637X/811/1/24
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU4BR
UT WOS:000363471600025
ER
PT J
AU Tao, L
Tomsick, JA
Walton, DJ
Furst, F
Kennea, J
Miller, JM
Boggs, SE
Christensen, FE
Craig, WW
Gandhi, P
Grefenstette, BW
Hailey, CJ
Harrison, FA
Krimm, HA
Pottschmidt, K
Stern, D
Tendulkar, SP
Zhang, WW
AF Tao, Lian
Tomsick, John A.
Walton, Dominic J.
Fuerst, Felix
Kennea, Jamie
Miller, Jon M.
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Gandhi, Poshak
Grefenstette, Brian W.
Hailey, Charles J.
Harrison, Fiona A.
Krimm, Hans A.
Pottschmidt, Katja
Stern, Daniel
Tendulkar, Shriharsh P.
Zhang, William W.
TI NuSTAR AND SWIFT OBSERVATIONS OF THE BLACK HOLE CANDIDATE XTE J1908+094
DURING ITS 2013 OUTBURST
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; stars: individual (XTE
J1908+094); X-rays: binaries
ID X-RAY JETS; GX 339-4; RADIO-EMISSION; ACCRETION DISK; CYGNUS X-1;
REFLECTION; STATE; MODEL; LINES; SPIN
AB The black hole (BH) candidate XTE J1908+094 went into outburst for the first time since 2003 in 2013 October. We report on an observation with the Nuclear Spectroscopic Telescope Array (NuSTAR) and monitoring observations with Swift during the outburst. NuSTAR caught the source in the soft state: the spectra show a broad relativistic iron line, and the light curves reveal a similar to 40 ks flare, with the count rate peaking about 40% above the non-flare level and with significant spectral variation. A model combining a multi-temperature thermal component, a power law, and a reflection component with an iron line provides a good description of the NuSTAR spectrum. Although relativistic broadening of the iron line is observed, it is not possible to constrain the BH spin with these data. The variability of the power-law component, which can also be modeled as a Comptonization component, is responsible for the flux and spectral change during the flare, suggesting that changes in the corona (or possibly continued jet activity) are the likely cause of the flare.
C1 [Tao, Lian; Walton, Dominic J.; Fuerst, Felix; Grefenstette, Brian W.; Harrison, Fiona A.; Tendulkar, Shriharsh P.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Tao, Lian] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China.
[Tao, Lian] Tsinghua Univ, Ctr Astrophys, Beijing 100084, Peoples R China.
[Tomsick, John A.; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Walton, Dominic J.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kennea, Jamie] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Gandhi, Poshak] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Gandhi, Poshak] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Krimm, Hans A.; Pottschmidt, Katja; Zhang, William W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Krimm, Hans A.] USRA, Columbia, MD 21044 USA.
[Pottschmidt, Katja] UMBC, CRESST, Dept Phys, Baltimore, MD 21250 USA.
[Pottschmidt, Katja] UMBC, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
RP Tao, L (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 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).
NR 48
TC 3
Z9 3
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2015
VL 811
IS 1
AR 51
DI 10.1088/0004-637X/811/1/51
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU4BR
UT WOS:000363471600052
ER
PT J
AU Venturelli, D
Mandra, S
Knysh, S
O'Gorman, B
Biswas, R
Smelyanskiy, V
AF Venturelli, Davide
Mandra, Salvatore
Knysh, Sergey
O'Gorman, Bryan
Biswas, Rupak
Smelyanskiy, Vadim
TI Quantum Optimization of Fully Connected Spin Glasses
SO PHYSICAL REVIEW X
LA English
DT Article
ID QUBITS; MODEL
AB Many NP-hard problems can be seen as the task of finding a ground state of a disordered highly connected Ising spin glass. If solutions are sought by means of quantum annealing, it is often necessary to represent those graphs in the annealer's hardware by means of the graph-minor embedding technique, generating a final Hamiltonian consisting of coupled chains of ferromagnetically bound spins, whose binding energy is a free parameter. In order to investigate the effect of embedding on problems of interest, the fully connected Sherrington-Kirkpatrick model with random +/- 1 couplings is programmed on the D-Wave Two (TM) annealer using up to 270 qubits interacting on a Chimera-type graph. We present the best embedding prescriptions for encoding the Sherrington-Kirkpatrick problem in the Chimera graph. The results indicate that the optimal choice of embedding parameters could be associated with the emergence of the spin-glass phase of the embedded problem, whose presence was previously uncertain. This optimal parameter setting allows the performance of the quantum annealer to compete with (and potentially outperform, in the absence of analog control errors) optimized simulated annealing algorithms.
C1 [Venturelli, Davide; Mandra, Salvatore; Knysh, Sergey; O'Gorman, Bryan; Biswas, Rupak] NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab QuAIL, Moffett Field, CA 94035 USA.
[Venturelli, Davide] USRA, Res Inst Adv Comp Sci, Mountain View, CA 94043 USA.
[Mandra, Salvatore] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02139 USA.
[Knysh, Sergey] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA.
[Smelyanskiy, Vadim] Google, Venice, CA 90291 USA.
RP Venturelli, D (reprint author), NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab QuAIL, Mail Stop 269-1, Moffett Field, CA 94035 USA.
EM davide.venturelli@nasa.gov
FU NASA [NNX14AF62G, NNX12AK33A]; Office of the Director of National
Intelligence (ODNI), Intelligence Advanced Research Projects Activity
(IARPA) [IAA 145483]; AFRL Information Directorate [F4HBKC4162G001]
FX We acknowledge useful discussions with Dr. Trevor Lanting, Dr. Andrew
King, Dr. Alejandro Perdomo-Ortiz, Dr. Eleanor G. Rieffel, Professor M.
Troyer, and Professor H. Katzgraber. Part of the work was supported by
NASA (Sponsor Awards No. NNX14AF62G and No. NNX12AK33A). The numerical
work was supported by the Office of the Director of National
Intelligence (ODNI), Intelligence Advanced Research Projects Activity
(IARPA), via IAA 145483, and by the AFRL Information Directorate under
Grant No. F4HBKC4162G001.
NR 43
TC 23
Z9 23
U1 1
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2160-3308
J9 PHYS REV X
JI Phys. Rev. X
PD SEP 18
PY 2015
VL 5
IS 3
AR 031040
DI 10.1103/PhysRevX.5.031040
PG 8
WC Physics, Multidisciplinary
SC Physics
GA CR5IR
UT WOS:000361375100002
ER
PT J
AU Tsuda, T
Shepherd, M
Gopalswamy, N
AF Tsuda, Toshitaka
Shepherd, Marianna
Gopalswamy, Nat
TI Advancing the understanding of the Sun-Earth interaction-the Climate and
Weather of the Sun-Earth System (CAWSES) II program
SO PROGRESS IN EARTH AND PLANETARY SCIENCE
LA English
DT Review
DE Coupled solar-terrestrial system; Solar activity; Space weather;
Geospace; Atmospheric coupling; Trends; Global warming; Paleoclimatology
ID GEOMAGNETIC-ACTIVITY; TEMPERATURE; VARIABILITY; MODEL
AB The Scientific Committee on Solar-Terrestrial Physics (SCOSTEP) of the International Council for Science (ICSU) implemented an international collaborative program called Climate and Weather of the Sun-Earth System (CAWSES), which was active from 2004 to 2008; this was followed by the CAWSES II program during the period of 2009-2013. The CAWSES program was aimed at improving the understanding of the coupled solar-terrestrial system, with special emphasis placed on the short-term (weather) and long-term (climate) variability of solar activities and their effects on and responses of Geospace and Earth's environment. Following the successful implementation of CAWSES, the CAWSES II program pursued four fundamental questions addressing the way in which the coupled Sun-Earth system operates over time scales ranging from minutes to millennia, namely, (1) What are the solar influences on the Earth's climate? (2) How will Geospace respond to an altered climate? (3) How does short-term solar variability affect the Geospace environment? and (4) What is the Geospace response to variable inputs from the lower atmosphere? In addition to these four major tasks, the SCOSTEP and CAWSES promoted E-science and informatics activities including the creation of scientific databases and their effective utilization in solar-terrestrial physics research. Capacity building activities were also enhanced during CAWSES II, and this represented an important contribution of SCOSTEP to the world's solar-terrestrial physics community. This introductory paper provides an overview of CAWSES II activities and serves as a preface to the dedicated review papers summarizing the achievements of the program's four task groups (TGs) and the E-science component.
C1 [Tsuda, Toshitaka] Kyoto Univ, Res Inst Sustainable Humanosphere, Kyoto 6110011, Japan.
[Shepherd, Marianna] York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 2R7, Canada.
[Gopalswamy, Nat] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Div, Greenbelt, MD 20771 USA.
RP Tsuda, T (reprint author), Kyoto Univ, Res Inst Sustainable Humanosphere, Kyoto 6110011, Japan.
EM tsuda@rish.kyoto-u.ac.jp
NR 23
TC 3
Z9 3
U1 1
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 2197-4284
J9 PROG EARTH PLANET SC
JI Prog. Earth Planet. Sci.
PD SEP 17
PY 2015
VL 2
AR 28
DI 10.1186/s40645-015-0059-0
PG 18
WC Geosciences, Multidisciplinary
SC Geology
GA CV0ND
UT WOS:000363946500002
ER
PT J
AU Godfroy-Cooper, M
Sandor, PMB
Miller, JD
Welch, RB
AF Godfroy-Cooper, Martine
Sandor, Patrick M. B.
Miller, Joel D.
Welch, Robert B.
TI The interaction of vision and audition in two-dimensional space
SO FRONTIERS IN NEUROSCIENCE
LA English
DT Article
DE visual-auditory; localization; precision; accuracy; 2D; MLE
ID PRIMATE SUPERIOR COLLICULUS; HUMAN SOUND LOCALIZATION; CROSS-MODAL BIAS;
HUMAN LISTENERS; AUDITORY SIGNALS; HEAD POSITION; EYE POSITION; VISUAL
SPACE; INTEGRATION; SACCADES
AB Using a mouse-driven visual pointer, 10 participants made repeated open-loop egocentric localizations of memorized visual, auditory, and combined visual-auditory targets projected randomly across the two-dimensional frontal field (2D). The results are reported in terms of variable error, constant error and local distortion. The results confirmed that auditory and visual maps of the egocentric space differ in their precision (variable error) and accuracy (constant error), both from one another and as a function of eccentricity and direction within a given modality. These differences were used, in turn, to make predictions about the precision and accuracy within which spatially and temporally congruent bimodal visual-auditory targets are localized. Overall, the improvement in precision for bimodal relative to the best unimodal target revealed the presence of optimal integration well-predicted by the Maximum Likelihood Estimation (MLE) model. Conversely, the hypothesis that accuracy in localizing the bimodal visual-auditory targets would represent a compromise between auditory and visual performance in favor of the most precise modality was rejected. Instead, the bimodal accuracy was found to be equivalent to or to exceed that of the best unimodal condition. Finally, we described how the different types of errors could be used to identify properties of the internal representations and coordinate transformations within the central nervous system (CNS). The results provide some insight into the structure of the underlying sensorimotor processes employed by the brain and confirm the usefulness of capitalizing on naturally occurring differences between vision and audition to better understand their interaction and their contribution to multimodal perception.
C1 [Godfroy-Cooper, Martine; Miller, Joel D.; Welch, Robert B.] NASA, Adv Controls & Displays Grp, Human Syst Integrat Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Godfroy-Cooper, Martine; Miller, Joel D.] San Jose State Univ, Res Fdn, San Jose, CA 95192 USA.
[Sandor, Patrick M. B.] Inst Rech Biomed Armees, Dept Act & Cognit Situat Operat, Bretigny Sur Orge, France.
[Sandor, Patrick M. B.] Aix Marseille Univ, CNRS, ISM UMR 7287, Marseille, France.
RP Godfroy-Cooper, M (reprint author), NASA, Ames Res Ctr, POB 1,Mail Stop 262-4, Moffett Field, CA 94035 USA.
EM martine.godfroy-1@nasa.gov
FU Direction Generale de l'Armement/Service de Sante des Armees grant; NASA
grant
FX We wish to thank C. Roumes for initial contribution, A. Bichot for
software development, R. Bittner for mathematical support and the
reviewers for their very helpful comments. A preliminary version of some
of the contents of this article is contained in the Proceedings of the
26th European Conference on Visual Perception and in the Proceedings of
the 26th Annual Meeting of the Cognitive Science Society. This work was
supported by a Direction Generale de l'Armement/Service de Sante des
Armees grant and a NASA grant.
NR 76
TC 0
Z9 0
U1 4
U2 13
PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
SN 1662-453X
J9 FRONT NEUROSCI-SWITZ
JI Front. Neurosci.
PD SEP 17
PY 2015
VL 9
AR 311
DI 10.3389/fnins.2015.00311
PG 18
WC Neurosciences
SC Neurosciences & Neurology
GA CS6SK
UT WOS:000362211700001
PM 26441492
ER
PT J
AU Jensen, BD
Wise, KE
Odegard, GM
AF Jensen, Benjamin D.
Wise, Kristopher E.
Odegard, Gregory M.
TI Simulation of the Elastic and Ultimate Tensile Properties of Diamond,
Graphene, Carbon Nanotubes, and Amorphous Carbon Using a Revised ReaxFF
Parametrization
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article; Proceedings Paper
CT 70th International Symposium on Molecular Spectroscopy
CY JUN 22-26, 2015
CL Champaign, IL
ID REACTIVE FORCE-FIELD; AUGMENTED-WAVE METHOD; MOLECULAR-DYNAMICS;
MECHANICAL-PROPERTIES; MONOLAYER GRAPHENE; STRENGTH; SCATTERING;
MODULUS; FILMS; DISPERSION
AB In light of the enduring interest in using nanostructured carbon materials as reinforcing elements in composite materials, there is a significant need for a reliable computational tool capable to predict the mechanical properties, both elastic properties and properties at the point of fracture, in large-scale atomistic simulations. A revised version of the ReaxFF reactive force field parametrization for carbon, ReaxFF(C-2013), was recently published and is notable because of the inclusion of density functional theory (DFT)-derived mechanical data for diamond and graphite in the fitting set. The purpose of the present work is to assess the accuracy of this new force field for predicting the mechanical properties for several allotropes of carbon, both in the elastic regime and during fracture. The initial discussion focuses on the performance of ReaxFF(C-2013) for diamond and graphene, the two carbon forms for which mechanical properties were included in the parametrization data set. After it is established that simulations conducted with the new force field yield results that agree well with DFT and experimental data for most properties of interest, its transferability to amorphous carbon and carbon nanotubes is explored. ReaxFF(C-2013) is found to produce results that, for the most part, compare favorably with available experimental data for single and multiwalled nanotubes and for amorphous carbon models prepared over a range of densities. Although there is opportunity for improvement in some predicted properties, the ReaxFF(C-2013) parametrization is shown to generally perform well for each form of carbon and to compare favorably with DFT and experimental data.
C1 [Jensen, Benjamin D.; Wise, Kristopher E.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Jensen, Benjamin D.; Odegard, Gregory M.] Michigan Technol Univ, Dept Mech Engn Engn Mech, Houghton, MI 49931 USA.
EM gmodegar@mtu.edu
RI Jensen, Benjamin/B-1297-2013
OI Jensen, Benjamin/0000-0002-7982-0663
FU NASA under the Revolutionary Technology Challenges Program [NNX09AM50A]
FX This research was funded by NASA under the Revolutionary Technology
Challenges Program (Grant NNX09AM50A). SUPERIOR, a high-performance
computing cluster at Michigan Technological University, was used in
obtaining some of results presented in this publication.
NR 55
TC 6
Z9 6
U1 10
U2 50
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD SEP 17
PY 2015
VL 119
IS 37
BP 9710
EP 9721
DI 10.1021/acs.jpca.5b05889
PG 12
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA CS1ZL
UT WOS:000361867500018
PM 26315717
ER
PT J
AU Bloomberg, JJ
Peters, BT
Cohens, HS
Mulavara, AP
AF Bloomberg, Jacob J.
Peters, Brian T.
Cohens, Helen S.
Mulavara, Ajitkumar P.
TI Enhancing astronaut performance using sensorimotor adaptability training
SO FRONTIERS IN SYSTEMS NEUROSCIENCE
LA English
DT Review
DE spaceflight; countermeasures; training; motor learning; plasticity
ID FUNCTIONAL ANKLE INSTABILITY; LONG-DURATION SPACEFLIGHT; NEUROMUSCULAR
ACTIVATION PATTERNS; STOCHASTIC RESONANCE STIMULATION; SPACE SUIT
BIOENERGETICS; VIRTUAL-REALITY; VARIABLE PRACTICE; MOTOR SKILL;
CONTEXTUAL INTERFERENCE; OBSTACLE AVOIDANCE
AB Astronauts experience disturbances in balance and gait function when they return to Earth. The highly plastic human brain enables individuals to modify their behavior to match the prevailing environment. Subjects participating in specially designed variable sensory challenge training programs can enhance their ability to rapidly adapt to novel sensory situations. This is useful in our application because we aim to train astronauts to rapidly formulate effective strategies to cope with the balance and locomotor challenges associated with new gravitational environments enhancing their ability to "learn to learn." We do this by coupling various combinations of sensorimotor challenges with treadmill walking. A unique training system has been developed that is comprised of a treadmill mounted on a motion base to produce movement of the support surface during walking. This system provides challenges to gait stability. Additional sensory variation and challenge are imposed with a virtual visual scene that presents subjects with various combinations of discordant visual information during treadmill walking. This experience allows them to practice resolving challenging and conflicting novel sensory information to improve their ability to adapt rapidly. Information obtained from this work will inform the design of the next generation of sensorimotor countermeasures for astronauts.
C1 [Bloomberg, Jacob J.] NASA, Johnson Space Ctr, Neurosci Labs, Biomed Res & Environm Sci Div, Houston, TX 77058 USA.
[Peters, Brian T.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Cohens, Helen S.] Baylor Coll Med, Bobby R Alford Dept Otolaryngol Head & Neck Surg, Houston, TX 77030 USA.
[Mulavara, Ajitkumar P.] Univ Space Res Assoc, Houston, TX USA.
RP Bloomberg, JJ (reprint author), NASA, Johnson Space Ctr, Neurosci Labs, Biomed Res & Environm Sci Div, Mail Code SK272, Houston, TX 77058 USA.
EM Jacob.j.bloomberg@nasa.gov
NR 137
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Z9 1
U1 4
U2 9
PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
SN 1662-5137
J9 FRONT SYST NEUROSCI
JI Front. Syst. Neurosci.
PD SEP 16
PY 2015
VL 9
AR 129
DI 10.3389/fnsys.2015.00129
PG 12
WC Neurosciences
SC Neurosciences & Neurology
GA CU9GN
UT WOS:000363852800001
PM 26441561
ER
PT J
AU Li, W
Thorne, RM
Bortnik, J
Baker, DN
Reeves, GD
Kanekal, SG
Spence, HE
Green, JC
AF Li, W.
Thorne, R. M.
Bortnik, J.
Baker, D. N.
Reeves, G. D.
Kanekal, S. G.
Spence, H. E.
Green, J. C.
TI Solar wind conditions leading to efficient radiation belt electron
acceleration: A superposed epoch analysis
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID WHISTLER-MODE CHORUS; VAN ALLEN PROBES; RELATIVISTIC ELECTRONS; MAGNETIC
STORMS; GEOMAGNETIC STORMS; SEED POPULATION; PC5 WAVES; MAGNETOSPHERE;
EVENT; ZONE
AB Determining preferential solar wind conditions leading to efficient radiation belt electron acceleration is crucial for predicting radiation belt electron dynamics. Using Van Allen Probes electron observations (>1 MeV) from 2012 to 2015, we identify a number of efficient and inefficient acceleration events separately to perform a superposed epoch analysis of the corresponding solar wind parameters and geomagnetic indices. By directly comparing efficient and inefficient acceleration events, we clearly show that prolonged southward B-z, high solar wind speed, and low dynamic pressure are critical for electron acceleration to >1 MeV energies in the heart of the outer radiation belt. We also evaluate chorus wave evolution using the superposed epoch analysis for the identified efficient and inefficient acceleration events and find that chorus wave intensity is much stronger and lasts longer during efficient electron acceleration events, supporting the scenario that chorus waves play a key role in MeV electron acceleration.
C1 [Li, W.; Thorne, R. M.; Bortnik, J.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[Baker, D. N.] Univ Colorado, Lab Atmospher & Space Res, Boulder, CO 80309 USA.
[Reeves, G. D.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM USA.
[Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Green, J. C.] Space Hazard Applicat LLC, Golden, CO USA.
RP Li, W (reprint author), Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
EM moonli@atmos.ucla.edu
RI Reeves, Geoffrey/E-8101-2011
OI Reeves, Geoffrey/0000-0002-7985-8098
FU JHU/APL under NASA [967399, 921647, NAS5-01072]; ECT [13-041]; NASA
[NNX11AD75G, NNX14AN85G, NNX11AR64G, NNX13AI61G]; Air Force Young
Investigator program [FA9550-15-1-0158]
FX This work was supported by JHU/APL contracts 967399 and 921647 under
NASA's prime contract NAS5-01072. The analysis at UCLA was supported by
the ECT subaward 13-041, NASA grants NNX11AD75G, NNX14AN85G, NNX11AR64G,
and NNX13AI61G, and the Air Force Young Investigator program
FA9550-15-1-0158. We acknowledge the Van Allen Probes data from the REPT
and MagEIS instruments obtained from
http://www.rbsp-ect.lanl.gov/data_pub/. We greatly appreciate the NOAA
POES data obtained from http://satdat.ngdc.noaa.gov/sem/poes/data/ and
the NOAA POES team for providing helpful advice. We also thank the World
Data Center for Geomagnetism, Kyoto for providing SYM-H and AL indices
(http://wdc.kugi.kyoto-u.ac.jp/aeasy/index.html), and the Space Physics
Data Facility at the NASA Goddard Space Flight Center for providing the
OMNI2 data (ftp://spdf.gsfc.nasa.gov/pub/data/omni/omni_c-daweb/).
NR 56
TC 6
Z9 6
U1 2
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 16
PY 2015
VL 42
IS 17
BP 6906
EP 6915
DI 10.1002/2015GL065342
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GB
UT WOS:000363411200005
ER
PT J
AU Ngwira, CM
Pulkkinen, AA
Bernabeu, E
Eichner, J
Viljanen, A
Crowley, G
AF Ngwira, Chigomezyo M.
Pulkkinen, Antti A.
Bernabeu, Emanuel
Eichner, Jan
Viljanen, Ari
Crowley, Geoff
TI Characteristics of extreme geoelectric fields and their possible causes:
Localized peak enhancements
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GEOMAGNETICALLY INDUCED CURRENTS; 29-31 OCTOBER 2003; PLASMA SHEET;
SCENARIOS; SYSTEMS; EVENTS
AB One of the major challenges pertaining to extreme geomagnetic storms is to understand the basic processes associated with the development of dynamic magnetosphere-ionosphere currents, which generate large induced surface geoelectric fields. Previous studies point out the existence of localized peak geoelectric field enhancements during extreme storms. We examined induced global geoelectric fields derived from ground-based magnetometer recordings for 12 extreme geomagnetic storms between the years 1982 and 2005. For the present study two important extreme storms, 29 October 2003 and 13 March 1989, are shown. The primary purpose of this paper is to provide further evidence on the existence of localized peak geoelectric field enhancements and to show that the structure of the geoelectric field during these localized extremes at single sites can differ greatly from globally and regionally averaged fields. Although the physical processes that govern the development of these localized extremes are still not clear, we discuss some possible causes.
C1 [Ngwira, Chigomezyo M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Ngwira, Chigomezyo M.; Pulkkinen, Antti A.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
[Bernabeu, Emanuel] PJM Interconnect, Audubon, PA USA.
[Eichner, Jan] Munich Re, Geo Risks Res, Munich, Germany.
[Viljanen, Ari] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Crowley, Geoff] Atmospher & Space Technol Res Associates, Boulder, CO USA.
RP Ngwira, CM (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
EM chigomezyo.ngwira@nasa.gov
FU NASA [NNG11PL10A 670.035]; ASTRA [ASTRA-2014-02]
FX We thank the national institutes that support magnetic observatories and
INTERMAGNET for promoting high standards of magnetic observatory
practice. Valuable discussions with Eftyhia Zesta are gratefully
acknowledged. The work by C.M.N. was supported by NASA grant NNG11PL10A
670.035 to CUA/IACS and partly by ASTRA IR and D funds (grant
ASTRA-2014-02 to CUA/IACS).
NR 20
TC 8
Z9 8
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 16
PY 2015
VL 42
IS 17
BP 6916
EP 6921
DI 10.1002/2015GL065061
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GB
UT WOS:000363411200006
ER
PT J
AU Fatemi, S
Fuqua, HA
Poppe, AR
Delory, GT
Halekas, JS
Farrell, WM
Holmstrom, M
AF Fatemi, S.
Fuqua, H. A.
Poppe, A. R.
Delory, G. T.
Halekas, J. S.
Farrell, W. M.
Holmstrom, M.
TI On the confinement of lunar induced magnetic fields
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SOLAR-WIND INTERACTION; ELECTRICAL-CONDUCTIVITY; ELECTROMAGNETIC
INDUCTION; SEISMIC DATA; MOON; INTERIOR; CORE; MAGNETOMETER; WAKE;
INVERSION
AB We examine the confinement of induced magnetic fields on the lunar dayside and nightside, when the Moon is in the solar wind. We use a three-dimensional hybrid model of plasma and place a dipole magnetic field at the center of the Moon to mimic the induced magnetic field, which is the response of the lunar interior to the time-varying interplanetary magnetic field. Consistent with previous observations and theoretical predictions, we show that the induced magnetic fields on the dayside are confined within the lunar surface through a dayside current sheet. In contrast to previous work, we show that the induced magnetic fields are not confined in the lunar wake, and they leak out, sometimes even appearing as lunar limb compressions. Finally, we identify favorable places to observe induced magnetic fields by electromagnetic sounding techniques, which will help to better constrain the lunar electrical conductivity profile, and interior structure.
C1 [Fatemi, S.; Fuqua, H. A.; Poppe, A. R.; Delory, G. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Fatemi, S.; Fuqua, H. A.; Poppe, A. R.; Delory, G. T.; Halekas, J. S.; Farrell, W. M.] NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA.
[Halekas, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Holmstrom, M.] Swedish Inst Space Phys, S-98128 Kiruna, Sweden.
RP Fatemi, S (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM shahab@ssl.berkeley.edu
RI Farrell, William/I-4865-2013;
OI Poppe, Andrew/0000-0001-8137-8176; Holmstrom, Mats/0000-0001-5494-5374;
Halekas, Jasper/0000-0001-5258-6128
FU NASA's SSERVI institute [NNX14AG16A]; NASA Earth and Space Science
Fellowship Program [NESSF15]
FX S.F., H.A.F., A.R.P., G.T.D., J.S.H., and W.M.F. gratefully acknowledge
support from NASA's SSERVI institute, grant NNX14AG16A. H.A.F. work was
also supported by NASA Earth and Space Science Fellowship Program, grant
NESSF15. This publication is a SSERVI contribution SSERVI-2015-161. This
research was conducted using resources provided by the Swedish National
Infrastructure for Computing (SNIC) at the High Performance Computing
Center North (HPC2N), Umea University, Sweden. The software used in this
work was developed in part by the DOE NNSA ASC-supported and DOE Office
of Science ASCR-supported Flash Center for Computational Science at the
University of Chicago. All ARTEMIS data used here are publicly available
at http://artemis.ssl.berkeley.edu and NASA's CDAWeb.
NR 45
TC 2
Z9 2
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 16
PY 2015
VL 42
IS 17
BP 6931
EP 6938
DI 10.1002/2015GL065576
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GB
UT WOS:000363411200008
ER
PT J
AU Soderblom, JM
Evans, AJ
Johnson, BC
Melosh, HJ
Miljkovic, K
Phillips, RJ
Andrews-Hanna, JC
Bierson, CJ
Head, JW
Milbury, C
Neumann, GA
Nimmo, F
Smith, DE
Solomon, SC
Sori, MM
Wieczorek, MA
Zuber, MT
AF Soderblom, Jason M.
Evans, Alexander J.
Johnson, Brandon C.
Melosh, H. Jay
Miljkovic, Katarina
Phillips, Roger J.
Andrews-Hanna, Jeffrey C.
Bierson, Carver J.
Head, James W., III
Milbury, Colleen
Neumann, Gregory A.
Nimmo, Francis
Smith, David E.
Solomon, Sean C.
Sori, Michael M.
Wieczorek, Mark A.
Zuber, Maria T.
TI The fractured Moon: Production and saturation of porosity in the lunar
highlands from impact cratering
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MASCON BASINS; GRAIL; POPULATIONS; CONSTRAINTS; DILATANCY; MISSION;
CRUST
AB We have analyzed the Bouguer anomaly (BA) of similar to 1200 complex craters in the lunar highlands from Gravity Recovery and Interior Laboratory observations. The BA of these craters is generally negative, though positive BA values are observed, particularly for smaller craters. Crater BA values scale inversely with crater diameter, quantifying how larger impacts produce more extensive fracturing and dilatant bulking. The Bouguer anomaly of craters larger than 93(19)(+47) km in diameter is independent of crater size, indicating that there is a limiting depth to impact-generated porosity, presumably from pore collapse associated with either overburden pressure or viscous flow. Impact-generated porosity of the bulk lunar crust is likely in a state of equilibrium for craters smaller than similar to 30 km in diameter, consistent with an similar to 8 km thick lunar megaregolith, whereas the gravity signature of larger craters is still preserved and provides new insight into the cratering record of even the oldest lunar surfaces.
C1 [Soderblom, Jason M.; Johnson, Brandon C.; Miljkovic, Katarina; Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Evans, Alexander J.; Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Melosh, H. Jay; Milbury, Colleen] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA.
[Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO USA.
[Andrews-Hanna, Jeffrey C.] Colorado Sch Mines, Dept Geophys, Golden, CO 80401 USA.
[Andrews-Hanna, Jeffrey C.] Colorado Sch Mines, Ctr Space Resources, Golden, CO 80401 USA.
[Bierson, Carver J.; Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Head, James W., III] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
[Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
[Sori, Michael M.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Wieczorek, Mark A.] Univ Paris Diderot, Inst Phys Globe Paris, Sorbonne Paris Cite, Paris, France.
RP Soderblom, JM (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
EM jms4@mit.edu
RI Neumann, Gregory/I-5591-2013; Wieczorek, Mark/G-6427-2010; Miljkovic,
Katarina/D-4844-2013;
OI Neumann, Gregory/0000-0003-0644-9944; Wieczorek,
Mark/0000-0001-7007-4222; Miljkovic, Katarina/0000-0001-8644-8903;
Soderblom, Jason/0000-0003-3715-6407; Bierson,
Carver/0000-0002-6840-7187; Sori, Michael/0000-0002-6191-2447
FU GRAIL mission - NASA Discovery Program
FX We thank all those involved with the development and operations of the
GRAIL spacecraft and the collection and reduction of the GRAIL data. We
also thank Sai Ravela (MIT) for his guidance with the statistical
analyses used in this paper. Gareth Collins and Boris Ivanov provided
constructive reviews that helped to improve this manuscript. This work
was funded by the GRAIL mission, which is supported by the NASA
Discovery Program, and is performed under contract to the Massachusetts
Institute of Technology and the Jet Propulsion Laboratory, California
Institute of Technology. Data used in this paper are archived in the
Geophysics Node of the Planetary Data System.
NR 33
TC 8
Z9 8
U1 2
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 16
PY 2015
VL 42
IS 17
BP 6939
EP 6944
DI 10.1002/2015GL065022
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GB
UT WOS:000363411200009
ER
PT J
AU Perry, ME
Neumann, GA
Phillips, RJ
Barnouin, OS
Ernst, CM
Kahan, DS
Solomon, SC
Zuber, MT
Smith, DE
Hauck, SA
Peale, SJ
Margot, JL
Mazarico, E
Johnson, CL
Gaskell, RW
Roberts, JH
McNutt, RL
Oberst, J
AF Perry, Mark E.
Neumann, Gregory A.
Phillips, Roger J.
Barnouin, Olivier S.
Ernst, Carolyn M.
Kahan, Daniel S.
Solomon, Sean C.
Zuber, Maria T.
Smith, David E.
Hauck, Steven A., II
Peale, Stanton J.
Margot, Jean-Luc
Mazarico, Erwan
Johnson, Catherine L.
Gaskell, Robert W.
Roberts, James H.
McNutt, Ralph L., Jr.
Oberst, Juergen
TI The low-degree shape of Mercury
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MESSENGER FLYBYS; GRAVITY-FIELD; TOPOGRAPHY; OCCULTATION; ORIENTATION;
ALTIMETRY; IMAGES; RADIUS; ORBIT; CORE
AB The shape of Mercury, particularly when combined with its geoid, provides clues to the planet's internal structure, thermal evolution, and rotational history. Elevation measurements of the northern hemisphere acquired by the Mercury Laser Altimeter on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging spacecraft, combined with 378 occultations of radio signals from the spacecraft in the planet's southern hemisphere, reveal the low-degree shape of Mercury. Mercury's mean radius is 2439.36 +/- 0.02 km, and there is a 0.14 km offset between the planet's centers of mass and figure. Mercury is oblate, with a polar radius 1.65 km less than the mean equatorial radius. The difference between the semimajor and semiminor equatorial axes is 1.25 km, with the long axis oriented 15 degrees west of Mercury's dynamically defined principal axis. Mercury's geoid is also oblate and elongated, but it deviates from a sphere by a factor of 10 less than Mercury's shape, implying compensation of elevation variations on a global scale.
C1 [Perry, Mark E.; Barnouin, Olivier S.; Ernst, Carolyn M.; Roberts, James H.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Neumann, Gregory A.; Mazarico, Erwan] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Phillips, Roger J.] Southwest Res Inst, Planetary Sci Directorate, Boulder, CO USA.
[Kahan, Daniel S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DE USA.
[Zuber, Maria T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA.
[Hauck, Steven A., II] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA.
[Peale, Stanton J.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Margot, Jean-Luc] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA.
[Johnson, Catherine L.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V5Z 1M9, Canada.
[Johnson, Catherine L.; Gaskell, Robert W.] Inst Plant Sci, Tucson, AZ USA.
[Oberst, Juergen] Inst Planetary Res, German Aerosp Ctr, Berlin, Germany.
[Oberst, Juergen] Moscow State Univ Geodesy & Cartog, MIIGAiK Extraterr Lab, Moscow, Russia.
RP Perry, ME (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
EM Mark.Perry@jhuapl.edu
RI Ernst, Carolyn/I-4902-2012; Roberts, James/I-9030-2012; Perry,
Mark/B-8870-2016; Barnouin, Olivier/I-7475-2015; Margot,
Jean-Luc/A-6154-2012; Neumann, Gregory/I-5591-2013; Mazarico,
Erwan/N-6034-2014;
OI Perry, Mark/0000-0003-1600-6856; Barnouin, Olivier/0000-0002-3578-7750;
Margot, Jean-Luc/0000-0001-9798-1797; Neumann,
Gregory/0000-0003-0644-9944; Mazarico, Erwan/0000-0003-3456-427X; Hauck,
Steven/0000-0001-8245-146X
FU NASA Discovery Program [NAS5-97271, NASW-00002]; MESSENGER Participating
Scientist Program; Russian Science Foundation [14-22-00197]; Natural
Sciences and Engineering Research Council of Canada
FX MESSENGER Radio Science and altimetry data are archived in the PDS
Geosciences Node http://pds-geosciences.wustl.edu. Details on MESSENGER
are maintained and updated at the MESSENGER website:
http://messenger.jhuapl.edu/. The MESSENGER mission 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, and the MESSENGER Participating Scientist
Program. Juergen Oberst was hosted by the Moscow State University for
Geodesy and Cartography (MIIGAiK) and supported by the Russian Science
Foundation, under project 14-22-00197. Catherine Johnson also
acknowledges support from the Natural Sciences and Engineering Research
Council of Canada.
NR 35
TC 5
Z9 5
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 16
PY 2015
VL 42
IS 17
BP 6951
EP 6958
DI 10.1002/2015GL065101
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GB
UT WOS:000363411200011
ER
PT J
AU Yue, J
Russell, J
Jian, YX
Rezac, L
Garcia, R
Lopez-Puertas, M
Mlynczak, MG
AF Yue, Jia
Russell, James, III
Jian, Yongxiao
Rezac, Ladislav
Garcia, Rolando
Lopez-Puertas, Manuel
Mlynczak, Martin G.
TI Increasing carbon dioxide concentration in the upper atmosphere observed
by SABER
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID TOTAL OZONE; CO2; THERMOSPHERE; MESOSPHERE; TRENDS
AB Carbon dioxide measurements made by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument between 2002 and 2014 were analyzed to reveal the rate of increase of CO2 in the mesosphere and lower thermosphere. The CO2 data show a trend of similar to 5% per decade at similar to 80 km and below, in good agreement with the tropospheric trend observed at Mauna Loa. Above 80 km, the SABER CO2 trend is larger than in the lower atmosphere, reaching similar to 12% per decade at 110 km. The large relative trend in the upper atmosphere is consistent with results from the Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE-FTS). On the other hand, the CO2 trend deduced from the Whole Atmosphere Community Climate Model remains close to 5% everywhere. The spatial coverage of the SABER instrument allows us to analyze the CO2 trend as a function of latitude for the first time. The trend is larger in the Northern Hemisphere than in the Southern Hemisphere mesopause above 80 km. The agreement between SABER and ACE-FTS suggests that the rate of increase of CO2 in the upper atmosphere over the past 13 years is considerably larger than can be explained by chemistry-climate models.
C1 [Yue, Jia; Russell, James, III; Jian, Yongxiao; Rezac, Ladislav] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Rezac, Ladislav] Max Planck Inst Solar Syst Res, Gottingen, Germany.
[Garcia, Rolando] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Lopez-Puertas, Manuel] CSIC, Inst Astrofis Andalucia, Granada, Spain.
[Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Yue, J (reprint author), Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
EM jia.yue@hamptonu.edu
RI Yue, Jia/D-8177-2011;
OI Lopez-Puertas, Manuel/0000-0003-2941-7734
FU NASA [NNX14AF20G, NNH13ZDA001N-HGI]; National Science Foundation;
Spanish MICINN [AYA2011-23552]; EC FEDER funds
FX We would like to acknowledge the hard work and support of the SABER
retrieval team who provided the version 2.0 data, including scientists
from GATS, Inc., NASA Langley Research Center, NASA Goddard Space Flight
Center, and Spain (IAA) and Arcon, Inc. We also would like to thank the
ACE-FTS team for providing the CO2 data. The SABER
CO2 data are now available to the public in the form of daily
NetCDF files at ftp://saber.gats-inc.com/Version2_0/Level2C/. The
ACE-FTS CO2 data (level 2, version 3.0) were downloaded from
http://www.ace.uwaterloo.ca/data.html. We are grateful to Kaley Walker
and Ryan Hughes for their assistance on the ACE-FTS data. More
information about WACCM can be found at
https://www2.acom.ucar.edu/gcm/waccm. The MERRA data can be obtained
from http://disc.sci.gsfc.nasa.gov/daac-bin/DataHoldings.pl. J.Y. is
supported by NASA grants NNX14AF20G and NNH13ZDA001N-HGI. The National
Center for Atmospheric Research is sponsored by the National Science
Foundation. IAA was supported by the Spanish MICINN under project
AYA2011-23552 and EC FEDER funds.
NR 27
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U1 10
U2 19
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 16
PY 2015
VL 42
IS 17
BP 7194
EP 7199
DI 10.1002/2015GL064696
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GB
UT WOS:000363411200041
ER
PT J
AU Zhu, LY
Fischer, EV
Payne, VH
Worden, JR
Jiang, Z
AF Zhu, Liye
Fischer, Emily V.
Payne, Vivienne H.
Worden, John R.
Jiang, Zhe
TI TES observations of the interannual variability of PAN over Northern
Eurasia and the relationship to springtime fires
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID PEROXYACETYL NITRATE PAN; TROPOSPHERIC EMISSION SPECTROMETER;
SATELLITE-OBSERVATIONS; SYSTEM; CHEMISTRY; OZONE
AB Peroxyacetyl nitrate (PAN) plays an important role in atmospheric chemistry through its impact on remote oxidant and nitrogen budgets. PAN is formed rapidly in boreal fire plumes through the oxidation of short-lived volatile organic compounds in the presence of nitrogen oxide radicals. Here we present new satellite observations of PAN from the Tropospheric Emission Spectrometer (TES) over northern Eurasia for April 2006-2010. We observe large interannual variability in TES PAN observations, and we show that fires are one source of this variability using (1) Moderate Resolution Imaging Spectroradiometer Mean Fire Radiative Power observations and (2) Hybrid Single-Particle Lagrangian Integrated Trajectory backward trajectories. We also show that cold springtime temperatures and enhanced vertical mixing in the lower free troposphere over northeastern Eurasia likely played a role in the detection of PAN from TES in April 2006 in this region.
C1 [Zhu, Liye; Fischer, Emily V.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Payne, Vivienne H.; Worden, John R.; Jiang, Zhe] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Zhu, LY (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
EM liyezhu@rams.colostate.edu
FU NASA [NNX14AF14G]
FX We acknowledge the MISR Science Team for the plume injection height
data, the Cloud Archive User Service (CLAUS) Project Team for the cloud
top brightness temperature data, and the TES Science Team for the TES
Lite products. Analyses and visualizations used in this study were
produced with the Giovanni online data system, developed and maintained
by the NASA GES DISC. Air temperature differences were diagnosed using
data from the NOAA/ESRL Physical Sciences Division, Boulder Colorado
(http://www.esrl.noaa.gov/psd/). We appreciate helpful discussions with
Elizabeth C. Weatherhead, Elizabeth A. Barnes, Peter Marinescu, and Sam
Atwood. This work was supported by NASA award NNX14AF14G. 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 26
TC 1
Z9 1
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 16
PY 2015
VL 42
IS 17
BP 7230
EP 7237
DI 10.1002/2015GL065328
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CU3GB
UT WOS:000363411200046
ER
PT J
AU Wang, SYS
Santanello, J
Wang, HL
Barandiaran, D
Pinker, RT
Schubert, S
Gillies, RR
Oglesby, R
Hilburn, K
Kilic, A
Houser, P
AF Wang, S. -Y. Simon
Santanello, Joseph
Wang, Hailan
Barandiaran, Daniel
Pinker, Rachel T.
Schubert, Siegfried
Gillies, Robert R.
Oglesby, Robert
Hilburn, Kyle
Kilic, Ayse
Houser, Paul
TI An intensified seasonal transition in the Central US that enhances
summer drought
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LOW-LEVEL JET; AMERICAN MONSOON SYSTEM; CENTRAL UNITED-STATES;
PRECIPITATION; VARIABILITY; REANALYSIS; TELECONNECTION; CIRCULATION;
PLAINS; TRENDS
AB In the long term, precipitation in the Central U.S. decreases by 25% during the seasonal transition from June to July. This precipitation decrease has intensified since 1979 and such intensification could have enhanced spring drought occurrences in the Central U.S., in which conditions quickly evolve from being abnormally dry to exceptionally dry. Various atmospheric and land reanalysis data sets were analyzed to examine the trend in the June-July seasonal transition. The intensified deficit in precipitation is accompanied by increased downward shortwave radiation flux, tropospheric subsidence, enhanced evaporative fraction, and elevated planetary boundary layer height, all of which can lead to surface drying. The change in tropospheric circulation was characterized by an anomalous ridge over the western U.S. and a trough on either side-a pattern known to suppress rainfall in the Central U.S. This trending pattern shows similarity with the progression of the 2012 record drought.
C1 [Wang, S. -Y. Simon; Barandiaran, Daniel; Gillies, Robert R.] Utah State Univ, Dept Plants Soils & Climate, Utah Climate Ctr, Logan, UT 84322 USA.
[Santanello, Joseph; Wang, Hailan; Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pinker, Rachel T.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Oglesby, Robert] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA.
[Hilburn, Kyle] Remote Sensing Syst, Santa Rosa, CA USA.
[Kilic, Ayse] Univ Nebraska, Dept Civil Engn, Lincoln, NE 68588 USA.
[Kilic, Ayse] Univ Nebraska, Sch Nat Resources, Lincoln, NE USA.
[Houser, Paul] George Mason Univ, Dept Geog & Geoinformat Sci, Fairfax, VA 22030 USA.
RP Wang, SYS (reprint author), Utah State Univ, Dept Plants Soils & Climate, Utah Climate Ctr, Logan, UT 84322 USA.
EM simon.wang@usu.edu
RI Santanello, Joseph/D-4438-2012
OI Santanello, Joseph/0000-0002-0807-6590
FU NASA; NASA MAP Program
FX This study was partially supported by the NASA Energy and Water cycle
Study. S. Schubert and H. Wang acknowledge support of the NASA MAP
Program. Global reanalysis products are provided at
http://gmao.gsfc.nasa.gov/research/merra/,
http://cfs.ncep.noaa.gov/cfsr/,
http://www.ecmwf.int/en/research/climate-reanalysis/era-interim,
http://www.esrl.noaa.gov/psd/data/reanalysis/reanalysis.shtml, and
http://www.esrl.noaa.gov/psd/data/gridded/data.narr.html. CRU
precipitation and surface air temperature data are provided at
http://www.cru.uea.ac.uk/data/, while the PDSI derived from PRISM is
provided at http://www.wrcc.dri.edu/wwdt/batchdownload.php. NLDAS-2 data
are provided at http://ldas.gsfc.nasa.gov/nldas/NLDAS2forcing.php. Model
AMIP simulations of FACTS are provided at
http://www.esrl.noaa.gov/psd/repository/alias/facts/.
NR 42
TC 4
Z9 4
U1 0
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 SEP 16
PY 2015
VL 120
IS 17
BP 8804
EP 8816
DI 10.1002/2014JD023013
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU3LB
UT WOS:000363425600013
ER
PT J
AU Strode, SA
Rodriguez, JM
Logan, JA
Cooper, OR
Witte, JC
Lamsal, LN
Damon, M
Van Aartsen, B
Steenrod, SD
Strahan, SE
AF Strode, Sarah A.
Rodriguez, Jose M.
Logan, Jennifer A.
Cooper, Owen R.
Witte, Jacquelyn C.
Lamsal, Lok N.
Damon, Megan
Van Aartsen, Bruce
Steenrod, Stephen D.
Strahan, Susan E.
TI Trends and variability in surface ozone over the United States
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID STRATOSPHERIC-TROPOSPHERIC TRANSPORT; INCREASING BACKGROUND OZONE;
AIR-QUALITY; NORTH-AMERICA; NOX EMISSIONS; POLLUTION EPISODES; SEASONAL
CYCLE; CLIMATE-CHANGE; GLOBAL-MODEL; RURAL-AREAS
AB We investigate the observed trends and interannual variability in surface ozone over the United States using the Global Modeling Initiative chemical transport model. We discuss the roles of meteorology, emissions, and transport from the stratosphere in driving the interannual variability in different regions and seasons. We demonstrate that a hindcast simulation for 1991-2010 can reproduce much of the observed variability and the trends in summertime ozone, with correlation coefficients for seasonally and regionally averaged median ozone ranging from 0.46 to 0.89. Reproducing the interannual variability in winter and spring in the western United States may require higher-resolution models to adequately represent stratosphere-troposphere exchange. Hindcast simulations with fixed versus variable emissions show that changes in anthropogenic emissions drive the observed negative trends in monthly median ozone concentrations in the eastern United States during summer, as well as the observed reduction in the amplitude of the seasonal cycle. The simulation underestimates positive trends in the western United States during spring, but excluding the first 4 years of data removes many of the statistically significant trends in this region. The reduction in the slope of the ozone versus temperature relationship before and after major emission reductions is also well represented by the model. Our results indicate that a global model can reproduce many of the important features of the meteorologically induced ozone variability as well as the emission-driven trends, lending confidence to model projections of future changes in regional surface ozone.
C1 [Strode, Sarah A.; Lamsal, Lok N.; Steenrod, Stephen D.; Strahan, Susan E.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Strode, Sarah A.; Rodriguez, Jose M.; Witte, Jacquelyn C.; Lamsal, Lok N.; Damon, Megan; Van Aartsen, Bruce; Steenrod, Stephen D.; Strahan, Susan E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Logan, Jennifer A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Cooper, Owen R.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO USA.
[Cooper, Owen R.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Witte, Jacquelyn C.; Damon, Megan; Van Aartsen, Bruce] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Strode, SA (reprint author), Univ Space Res Assoc, Columbia, MD 21044 USA.
EM sarah.a.strode@nasa.gov
RI Cooper, Owen/H-4875-2013; Strode, Sarah/H-2248-2012; Manager, CSD
Publications/B-2789-2015
OI Strode, Sarah/0000-0002-8103-1663;
FU NASA
FX This work was supported by NASA's Modeling, Analysis, and Prediction
program. The NASA High-End Computing Program provided resources to
support this work through the NASA Center for Climate Simulation at
Goddard Space Flight Center. GMI simulation results are available by
request to Susan Strahan (susan.e.strahan@nasa.gov). EPA CASTNET data,
OMI NO2 data, and MERRA data are available at
http://epa.gov/castnet/javaweb/index.html,
http://disc.sci.gsfc.nasa.gov/Aura/data-holdings/OMI/omno2_v003.shtml,
and http://disc.sci.gsfc.nasa.gov/daac-bin/DataHoldings.pl,
respectively.
NR 97
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Z9 15
U1 12
U2 55
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 16
PY 2015
VL 120
IS 17
BP 9020
EP 9042
DI 10.1002/2014JD022784
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU3LB
UT WOS:000363425600027
ER
PT J
AU Sha, J
Jo, YH
Oliver, MJ
Kohut, JT
Shatley, M
Liu, WT
Yan, XH
AF Sha, Jin
Jo, Young-Heon
Oliver, Matthew J.
Kohut, Josh T.
Shatley, Matthew
Liu, W. Timothy
Yan, Xiao-Hai
TI A case study of large phytoplankton blooms off the New Jersey coast with
multi-sensor observations
SO CONTINENTAL SHELF RESEARCH
LA English
DT Article
ID MID-ATLANTIC BIGHT; SURFACE WIND STRESS; RIVER PLUME; HEAT-FLUX;
CALIFORNIA; SHELF; CHLOROPHYLL; VARIABILITY; DYNAMICS; TEMPERATURE
AB Taking the 2111 summer bloom as a study case, we investigated the transport and nutrient delivery mechanisms for large phytoplankton blooms of the New Jersey coast. The horizontal advection of the chlorophyll is approximately one order larger than the horizontal diffusion averaging the whole study area. And the sea surface currents are found to correlate with the wind stress but only for part of the middle shelf. Based on the horizontal advection simulation driven by IF radar current, the bloom is divided into three sub-regions. The northern coastal section of the bloom shows high-low-high pattern in chlorophyll time series, which is related to coastal upwelling and a clockwise eddy. Coastal currents play an important role in the eddy formation and the southward transport of the bloom. The southern coastal section of the bloom is supported by the nutrients from coastal upwelling and driven offshore by wind. The northeast section of the bloom is fueled by nutrient source upwelled through Ekman pumping. The magnitude of Ekman pumping is of the same order as the magnitude of the upwelling along the coast. These identified mechanisms could also applied to more than half of bloom events during 2002 to 2013. In the summer of 2011 off the coast of New Jersey, processes in different sub-regions worked together, leading to this large phytoplanlcton bloom. (C) 2115 Elsevier Ltd. All rights reserved.
C1 [Sha, Jin; Jo, Young-Heon; Oliver, Matthew J.; Shatley, Matthew; Yan, Xiao-Hai] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA.
[Jo, Young-Heon] Pusan Natl Univ, Dept Oceanog, Busan, South Korea.
[Kohut, Josh T.] Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08903 USA.
[Liu, W. Timothy] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Yan, XH (reprint author), Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA.
EM xiaohai@udel.edu
FU China Scholarship Council; Long-term change of structure and function in
marine ecosystems of Korea - Ministry of Oceans and Fisheries, Korean;
NOAA Sea Grant [Na14OAR4170087]; NASA EPSCoR Program [NNX08AW02A]; NASA
Space Grant [NNG05G092H]
FX The authors thank the helpful discussions with colleagues in the Center
of Remote Sensing in University of Delaware. The first author of this
study, Jin Sha, was supported by the fellowship from China Scholarship
Council. YH Jo is supported by Long-term change of structure and
function in marine ecosystems of Korea, funded by the Ministry of Oceans
and Fisheries, Korean. The research work was also partially supported by
NOAA Sea Grant (Na14OAR4170087), NASA EPSCoR Program (NNX08AW02A) and
NASA Space Grant (NNG05G092H). This work benefited from helpful comments
provided by the editor and anonymous reviewers.
NR 54
TC 1
Z9 1
U1 2
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0278-4343
EI 1873-6955
J9 CONT SHELF RES
JI Cont. Shelf Res.
PD SEP 15
PY 2015
VL 107
BP 79
EP 91
DI 10.1016/j.csr.2015.07.006
PG 13
WC Oceanography
SC Oceanography
GA CS4MK
UT WOS:000362049700007
ER
PT J
AU Tompson, SR
AF Tompson, Sara R.
TI The Quotable Feynman
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Tompson, Sara R.] Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA.
RP Tompson, SR (reprint author), Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD SEP 15
PY 2015
VL 140
IS 15
BP 101
EP 101
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA CR5ZK
UT WOS:000361422700243
ER
PT J
AU Vadrevu, KP
Justice, C
Prasad, T
Prasad, N
Gutman, G
AF Vadrevu, Krishna Prasad
Justice, Chris
Prasad, Thenkabail
Prasad, Narasimha
Gutman, Garik
TI Land cover/land use change and impact on environment in South Asia -
(Continuation of January, 2015 special issue)
SO JOURNAL OF ENVIRONMENTAL MANAGEMENT
LA English
DT Editorial Material
C1 [Vadrevu, Krishna Prasad; Justice, Chris] Univ Maryland Coll Pk, Dept Geog Sci, College Pk, MD 20742 USA.
[Prasad, Thenkabail] US Geol Survey, Tempe, AZ USA.
[Prasad, Narasimha] Ctr Water Resources Dev & Management, Kozhikode, Kerala, India.
[Gutman, Garik] NASA Headquarters, Washington, DC USA.
RP Vadrevu, KP (reprint author), Univ Maryland Coll Pk, Dept Geog Sci, College Pk, MD 20742 USA.
NR 1
TC 0
Z9 0
U1 1
U2 12
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0301-4797
EI 1095-8630
J9 J ENVIRON MANAGE
JI J. Environ. Manage.
PD SEP 15
PY 2015
VL 161
BP 431
EP 432
DI 10.1016/j.jenvman.2015.07.054
PG 2
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA CR3WP
UT WOS:000361264100048
PM 26318499
ER
PT J
AU Montenbruck, O
Schmid, R
Mercier, F
Steigenberger, P
Noll, C
Fatkulin, R
Kogure, S
Ganeshan, AS
AF Montenbruck, O.
Schmid, R.
Mercier, F.
Steigenberger, P.
Noll, C.
Fatkulin, R.
Kogure, S.
Ganeshan, A. S.
TI GNSS satellite geometry and attitude models
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE GNSS satellites; Attitude models; Antenna offsets; ANTEX; SLR
ID YAW-ATTITUDE; GENERATION; RECEIVER; ANTENNAS; SYSTEMS; SERVICE
AB This article discusses the attitude modes employed by present Global (and Regional) Navigation Satellite Systems (GNSSs) and the models used to describe them along with definitions of the constellation-specific spacecraft body frames. A uniform convention for the labeling of the principal spacecraft axes is proposed by the International GNSS Service (IGS), which results in a common formulation of the nominal attitude of all GNSS satellites in yaw-steering mode irrespective of their specific orbit and constellation. The conventions defined within this document provide the basis for the specification of antenna phase center offsets and variations in a multi-GNSS version of the IGS absolute phase center model in the ANTEX (antenna exchange), format. To facilitate the joint analysis of GNSS observations and satellite laser ranging measurements, laser retroreflector array coordinates consistent with the IGS-specific spacecraft frame conventions are provided in addition to representative antenna offset values for all GNSS constellations. (C) 2015 COSPAR. Published by Elsevier Ltd. This is an open access article under the CC BY-NC-ND license (http://creativecommons.org/lic,enses/by-nc-nd/4.0/).
C1 [Montenbruck, O.; Steigenberger, P.] Deutsch Zentrum Luft & Raumfahrt DLR, GSOC, D-82234 Wessling, Germany.
[Schmid, R.] Tech Univ Munich, Deutsch Geodat Forschungsinst DGFI TUM, D-80333 Munich, Germany.
[Mercier, F.] CNES, F-31401 Toulouse 9, France.
[Noll, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fatkulin, R.] ISS Reshetnev, Zheleznogorsk 662972, Krasnoyarsk Reg, Russia.
[Kogure, S.] Japan Aerosp Explorat Agcy JAXA, Tsukuba Space Ctr, Tsukuba, Ibaraki 3058505, Japan.
[Ganeshan, A. S.] Indian Space Res Org, ISRO Satellite Ctr ISAC, Bangalore 560017, Karnataka, India.
RP Montenbruck, O (reprint author), Deutsch Zentrum Luft & Raumfahrt DLR, GSOC, D-82234 Wessling, Germany.
EM oliver.montenbruck@dlr.de; schmid@tum.de; flavien.mercier@cnes.fr;
peter.steigenberger@dlr.de; carey.noll@nasa.gov; frf@iss-reshetnev.ru;
kogure.satoshi@jaxa.jp; asganesh@isac.gov.in
RI Steigenberger, Peter/E-7500-2011; Schmid, Ralf/E-7484-2011
OI Steigenberger, Peter/0000-0003-1905-6699; Schmid,
Ralf/0000-0002-8794-2230
NR 68
TC 13
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U1 3
U2 16
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD SEP 15
PY 2015
VL 56
IS 6
BP 1015
EP 1029
DI 10.1016/j.asr.2015.06.019
PG 15
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CQ4TD
UT WOS:000360596600001
ER
PT J
AU Choi, J
Jo, JH
Roh, KM
Son, JY
Kim, MJ
Choi, YJ
Yim, HS
Moon, HK
Kim, BY
Park, JH
Pavlis, EC
AF Choi, Jin
Jo, Jung Hyun
Roh, Kyoung-Min
Son, Ju-Young
Kim, Myung-Jin
Choi, Young-Jun
Yim, Hong-Suh
Moon, Hong-Kyu
Kim, Bang-Yeop
Park, Jang-Hyun
Pavlis, Erricos C.
TI Analysis of the angle-only orbit determination for optical tracking
strategy of Korea GEO satellite, COMS
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE GEO; Optical tracking; Angle-only orbit determination; COMS; Sparse;
Dense
ID GEOSTATIONARY SATELLITE; IMPROVEMENT; ACCURACY
AB Increasing numbers of Geostationary Earth Orbit satellites have led to the requirement of accurate station keeping and precise orbit prediction to avoid collision between satellites. In the case of ground-based optical observation, angular resolution is better than other tracking systems, such as radar systems; however, the observation time of optical observation is limited by weather or lighting conditions. To develop an effective optical observation strategy, the optical observation campaign from January to February 2014 for Communication, Ocean and Meteorological Satellite (COMS) was conducted. Because COMS is a controlled satellite with station keeping manoeuvres performed twice a week, the observation results for 1- and 2-day observations were analysed. Sparse and sporadic cases for the sequential observation of multiple satellites and a dense case for the intensive observation of specific targets were assumed for the experiments. In the 1-day arc observation experiment, the estimated orbits for dense observation cases over 10% of the orbital period showed that the maximum difference was less than 40 km (station keeping area) for 7-day propagation compared to the estimation result using the whole 1-day measurement. For the 2-day arc observation, the orbit estimation difference could be maintained within 2 km using a more frequent observation than the 1-h interval for 13 h that was used in the sparse case. Additionally, the longitudinal and latitudinal positions via the estimation result using the optical observation were compared with the Two-Line Elements (TLEs) and operator's data. Through this study, an adequate optical tracking strategy was studied, and the possibility of cooperation with other systems was also validated. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Choi, Jin; Jo, Jung Hyun; Roh, Kyoung-Min; Son, Ju-Young; Kim, Myung-Jin; Choi, Young-Jun; Yim, Hong-Suh; Moon, Hong-Kyu; Park, Jang-Hyun] Korea Astron & Space Sci Inst, Space Situat Awareness Ctr, Taejon 305348, South Korea.
[Choi, Jin; Jo, Jung Hyun; Son, Ju-Young; Choi, Young-Jun] Korea Univ Sci & Technol, Taejon 305348, South Korea.
[Kim, Bang-Yeop] Korea Aerosp Res Inst, Geostationary Satellite Operat Team, Taejon 305600, South Korea.
[Jo, Jung Hyun; Pavlis, Erricos C.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA.
RP Jo, JH (reprint author), Korea Astron & Space Sci Inst, Space Situat Awareness Ctr, Taejon 305348, South Korea.
EM jhjo39@kasi.re.kr
FU National Research Council of Fundamental Science & Technology through a
National Agenda project "Development of Electro-optic Space Surveillance
System"; Korea Astronomy and Space Science Institute
FX This study was partially supported by the National Research Council of
Fundamental Science & Technology through a National Agenda project
"Development of Electro-optic Space Surveillance System" and the
matching fund from Korea Astronomy and Space Science Institute. Authors
also express sincere appreciation to colleagues for the development and
maintenance of the NESS system: Y.N. Yoon, S.Y. Yu, Y.H. Bae, Y.M. Lim,
S.Y. Park and W.Y. Han.
NR 31
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U1 1
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD SEP 15
PY 2015
VL 56
IS 6
BP 1056
EP 1066
DI 10.1016/j.asr.2015.06.005
PG 11
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CQ4TD
UT WOS:000360596600004
ER
PT J
AU Afshar-Mohajer, N
Wu, CY
Curtis, JS
Gaier, JR
AF Afshar-Mohajer, Nima
Wu, Chang-Yu
Curtis, Jennifer Sinclair
Gaier, James R.
TI Review of dust transport and mitigation technologies in lunar and
Martian atmospheres
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Electrical; Mechanical; Solar panel; Self-cleaning; Surface treatment
ID PARTICLE-SIZE DISTRIBUTION; TRAVELING-WAVE TRANSPORT; ELECTRIC CURTAIN;
ELECTRODYNAMIC SCREEN; REMOVAL EFFICIENCY; PLUME IMPINGEMENT; ROCKET
PLUME; SOLAR PANELS; MARS; EXPLORATION
AB Dust resuspension and deposition is a ubiquitous phenomenon in all lunar and Martian missions. The near-term plans to return to the Moon as a stepping stone to further exploration of Mars and beyond bring scientists' attention to development and evaluation of lunar and Martian dust mitigation technologies. In this paper, different lunar and Martian dust transport mechanisms are presented, followed by a review of previously developed dust mitigation technologies including fluidal, mechanical, electrical and passive self-cleaning methods for lunar/Martian installed surfaces along with filtration for dust control inside cabins. Key factors in choosing the most effective dust mitigation technology are recognized to be the dust transport mechanism, energy consumption, environment, type of surface materials, area of the surface and surface functionality. While electrical methods operating at higher voltages are identified to be suitable for small but light sensitive surfaces, pre-treatment of the surface is effective for cleaning thermal control surfaces, and mechanical methods are appropriate for surfaces with no concerns of light blockage, surface abrasion and 100% cleaning efficiency. Findings from this paper can help choose proper surface protection/cleaning for future space explorations. Hybrid techniques combining the advantages of different methods are recommended. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Afshar-Mohajer, Nima; Wu, Chang-Yu] Univ Florida, Dept Environm Engn Sci, Engn Sch Sustainable Infrastruct & Environm, Gainesville, FL 32611 USA.
[Curtis, Jennifer Sinclair] Univ Florida, Dept Chem Engn, Gainesville, FL 32611 USA.
[Gaier, James R.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Afshar-Mohajer, N (reprint author), Univ Florida, Dept Environm Engn Sci, POB 116450, Gainesville, FL 32611 USA.
EM nima.a-mohajer@jhu.edu
FU Space Research Initiative (SRI) [20040028, 20129027]
FX Partial financial support from the Space Research Initiative (SRI),
Grant Nos. 20040028 and 20129027, is greatly appreciated.
NR 115
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD SEP 15
PY 2015
VL 56
IS 6
BP 1222
EP 1241
DI 10.1016/j.asr.2015.06.007
PG 20
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CQ4TD
UT WOS:000360596600020
ER
PT J
AU Hochberg, EJ
Roberts, DA
Dennison, PE
Hulley, GC
AF Hochberg, Eric J.
Roberts, Dar A.
Dennison, Philip E.
Hulley, Glynn C.
TI Special issue on the Hyperspectral Infrared Imager (HyspIRI): Emerging
science in terrestrial and aquatic ecology, radiation balance and
hazards
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Hyperspectral Infrared Imager HyspIRI; Atmospheric correction;
Temperature; Emissivity; Terrestrial ecology; Aquatic ecology; Spectral
imaging
AB The Hyperspectral Infrared Imager (HyspIRI) mission is proposed to be the first satellite system with the capability to provide global, repeat coverage across the visible and shortwave infrared spectrum, as well as eight channels in the midwave and thermal infrared. HyspIRI has stated objectives to address a host of pressing earth science questions, from radiation budgets to ecosystem functions. A sizable science community has grown to support the mission, and their ongoing research demonstrates HyspIRI's potential to greatly expand our knowledge of the earth system. This special issue features a collection of papers, some reviews and others novel science, that cover the wide array of topics relevant to HyspIRI's mission and reaffirm the necessity for HyspIRI. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Hochberg, Eric J.] Bermuda Inst Ocean Sci, Biol Stn 17, St Georges GE01, Bermuda.
[Roberts, Dar A.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
[Dennison, Philip E.] Univ Utah, Dept Geog, Salt Lake City, UT 84112 USA.
[Hulley, Glynn C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hochberg, EJ (reprint author), Bermuda Inst Ocean Sci, Biol Stn 17, St Georges GE01, Bermuda.
EM eric.hochberg@bios.edu
OI Dennison, Philip/0000-0002-0241-1917
NR 24
TC 7
Z9 7
U1 5
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 SEP 15
PY 2015
VL 167
SI SI
BP 1
EP 5
DI 10.1016/j.rse.2015.06.011
PG 5
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CQ3OB
UT WOS:000360510800001
ER
PT J
AU Lee, CM
Cable, ML
Hook, SJ
Green, RO
Ustin, SL
Mandl, DJ
Middleton, EM
AF Lee, Christine M.
Cable, Morgan L.
Hook, Simon J.
Green, Robert O.
Ustin, Susan L.
Mandl, Daniel J.
Middleton, Elizabeth M.
TI An introduction to the NASA Hyperspectral InfraRed Imager (HyspIRI)
mission and preparatory activities
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Hyperspectral imager; Imaging spectroscopy; VSWIR; TIR; ECOSTRESS;
Decadal survey; Terrestrial ecology; Aquatic systems; Intelligent
payload module
ID IMAGING SPECTROMETER AVIRIS; EARTH OBSERVING ONE; REMOTE-SENSING
TECHNIQUES; LAND-SURFACE TEMPERATURE; ONE EO-1 SATELLITE;
GULF-OF-MEXICO; OCEAN COLOR; COASTAL WATERS; CHLOROPHYLL-A; RAIN-FORESTS
AB In 2007, the NASA Hyperspectral InfraRed Imager (HyspIRI) mission was recommended in Earth Science and Applications from Space: National Imperatives for the Next Decade and Beyond (Decadal Survey) to address critical science questions in multiple areas, in particular ecosystems and natural hazards. HyspIRI is comprised of two instruments, a visible to short-wavelength infrared (VSWIR) imaging spectrometer and a thermal infrared (TIR) multispectral imager, together with an Intelligent Payload Module (IPM) for onboard processing and rapid downlink of selected data. The VSWIR instrument will have 10 nm contiguous bands and cover the 380-2500 nm spectral range with 30 m spatial resolution and a revisit of 16 days. The TIR instrument will have 8 discrete bands in the 4-13 mu m range with 60 m spatial resolution and a revisit of 5 days. With these two instruments in low Earth orbit, HyspIRI will be able to address key science and applications questions in a wide array of fields, ranging from ecosystem function and diversity to human health and urbanization. (C) 2015 Elsevier Inc All rights reserved.
C1 [Lee, Christine M.; Cable, Morgan L.; Hook, Simon J.; Green, Robert O.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA.
[Ustin, Susan L.] Univ Calif Davis, Davis, CA 95616 USA.
[Mandl, Daniel J.; Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lee, CM (reprint author), 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM christine.m.lee@jpl.nasa.gov
RI Hook, Simon/D-5920-2016
OI Hook, Simon/0000-0002-0953-6165
FU NASA Earth Science Division
FX The authors would like to thank the reviewers for helpful comments. The
authors also gratefully acknowledge comments and feedback from Dar
Roberts, Eric Hochberg, and Phil Dennison. Funding for this work was
provided by the NASA Earth Science Division. Part of this work was
conducted at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA, and at the NASA Goddard Space
Flight Center.
NR 169
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U1 7
U2 52
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 15
PY 2015
VL 167
SI SI
BP 6
EP 19
DI 10.1016/j.rse.2015.06.012
PG 14
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CQ3OB
UT WOS:000360510800002
ER
PT J
AU Realmuto, VJ
Dennison, PE
Foote, M
Ramsey, MS
Wooster, MJ
Wright, R
AF Realmuto, V. J.
Dennison, P. E.
Foote, M.
Ramsey, M. S.
Wooster, M. J.
Wright, R.
TI Specifying the saturation temperature for the HyspIRI 4-mu m channel
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE HyspIRI; Wildland fires; Volcanoes; Mid-infrared remote sensing
ID ACTIVE FIRE DETECTION; SPECTRAL MIXTURE ANALYSIS; INFRARED
IMAGE-ANALYSIS; LAVA FLOWS; MOUNT-ETNA; THERMAL-ANALYSIS; LASCAR
VOLCANO; BIRD SATELLITE; TRMM VIRS; ERUPTION
AB The investigation of high-temperature natural phenomena, such as wildland fires and active lava flows, is a primary science objective for the proposed Hyperspectral Infrared Imager (HyspIRI) mission. Current planning for HyspIRI includes a mid-infrared (MIR) channel centered at 4 mu m that will allow measurement of radiance emitted from high-temperature targets. In this paper we present the results of a study to specify the saturation temperature for the MIR channel. This study was based on reviews of the literature, together with case studies of airborne and satellite-based data acquired over high-temperature targets. The spatial resolution of MIR radiance measurements is an important consideration in the remote sensing of high-temperature phenomena, due to the presence of materials at different temperatures within the area covered by an image pixel. The HyspIRI MIR channel will provide a spatial resolution of 60 m, which is similar to 40 times finer (in terms of area) than the finest spatial resolution provided by heritage instruments (370 m). This fine spatial resolution will increase the probability that high-temperature targets fill an image pixel and, therefore, the HyspIRI MIR channel will require a saturation temperature 2 to 4 times higher than the saturation limits of heritage instruments. Based on our study, we recommend a saturation temperature of 1200 K (927 degrees C). This recommendation accounts for the high temperatures expected for natural phenomena, expected performance of the MIR channel, and overlap in sensitivity between the MIR and thermal infrared (7.5-12 mu m) HyspIRI channels. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Realmuto, V. J.; Foote, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dennison, P. E.] Univ Utah, Salt Lake City, UT USA.
[Ramsey, M. S.] Univ Pittsburgh, Pittsburgh, PA USA.
[Wooster, M. J.] Kings Coll London, London WC2R 2LS, England.
[Wright, R.] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
RP Realmuto, VJ (reprint author), CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM vincent.j.realmuto@jpl.nasa.gov
OI Dennison, Philip/0000-0002-0241-1917
NR 81
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 15
PY 2015
VL 167
SI SI
BP 40
EP 52
DI 10.1016/j.rse.2015.04.028
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CQ3OB
UT WOS:000360510800005
ER
PT J
AU Grigsby, SP
Hulley, GC
Roberts, DA
Scheele, C
Ustin, SL
Alsina, MM
AF Grigsby, Shane P.
Hulley, Glynn C.
Roberts, Dar A.
Scheele, Christopher
Ustin, Susan L.
Alsina, Maria Mar
TI Improved surface temperature estimates with MASTER/AVIRIS sensor fusion
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Canopy temperature; Validation; Water vapor scaling; Land surface
temperature; HyspIRI; Thermal infrared; MASTER
ID IMAGING SPECTROMETER DATA; ATMOSPHERIC WATER-VAPOR; STRESS; LAND;
IRRIGATION; ALGORITHM; INDICATOR; RESPONSES; AVIRIS; LEAF
AB Land surface temperature (LST) is an important parameter in many ecological studies. The current Root Mean Square Error (RMSE) in standard MODIS and ASTER LST products is greater than 1 K, and for ASTER can be as large as 4 K for graybody pixels such as vegetation. Errors of 3 to 8 K have been observed for ASTER in humid conditions, making knowledge of atmospheric water vapor content critical in retrieving accurate LST. For this reason improved accuracy in LST measurements through the synthesis of visible-to-shortwave-infrared (VSWIR) derived water vapor maps and Thermal-Infrared (TIR) data is one goal of the Hyperspectral Infrared Imager, or HyspIRI, mission. The 2011 ER-2 Delano/Lost Hills flights acquired data with both the MODIS/ASTER Simulator (MASTER) and Airborne Visible InfraRed Imaging Spectrometer (AVIRIS) instruments flown concurrently. This study compares LST retrieval accuracies from the standard JPL MASTER temperature products produced using the temperature-emissivity separation (TES) algorithm, and the water vapor scaling (WVS) atmospheric correction method proposed for HyspIRI. The two retrieval methods are run both with and without high spatial resolution AVIRIS-derived water vapor maps to assess the improvement from VSWIR synthesis. We find improvement using VSWIR derived water vapor maps, with the WVS method being most accurate overall. For closed canopy agricultural vegetation we observed temperature retrieval RMSEs of 0.49 K and 0.70 K using the WVS method on MASTER data with and without AVIRIS derived water vapor, respectively. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Grigsby, Shane P.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Grigsby, Shane P.; Roberts, Dar A.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
[Hulley, Glynn C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Scheele, Christopher] Univ Wisconsin, Atmospher & Ocean Sci, Madison, WI 53706 USA.
[Ustin, Susan L.; Alsina, Maria Mar] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA.
RP Grigsby, SP (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
EM shane@geog.ucsb.edu
RI Alsina, Maria del Mar/C-2879-2009;
OI Alsina, Maria del Mar/0000-0001-5344-0980; Grigsby,
Shane/0000-0003-4904-7785
FU NASA Student Airborne Research Program (SARP) through the University of
North Dakota, NASA Ames Cooperative for Research in Earth Science and
Technology (ARC-CREST) [NNX12AD05A, NNX12AD05A-UND1]
FX The research described in this paper was initiated with support by the
NASA Student Airborne Research Program (SARP) through the University of
North Dakota as part of the NASA Ames Cooperative for Research in Earth
Science and Technology (ARC-CREST) Award Number NNX12AD05A, Sub-award
NNX12AD05A-UND1, and was carried out at the University of California
Santa Barbara. We gratefully thank both Rose Dominguez and Jeff Myers at
UARC for their assistance with MASTER calibration data, as well as Dr.
David R. Smart and the USDA Specialty Crops Research Initiative (SCRI)
headed by Dr. Patrick Brown (PI) for their role in collecting the ground
measurements at Delano Vineyards. In addition, we thank the two
anonymous reviewers for their helpful comments, which were instrumental
in adding additional clarity to many parts of this text.
NR 50
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 15
PY 2015
VL 167
SI SI
BP 53
EP 63
DI 10.1016/j.rse.2015.05.019
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CQ3OB
UT WOS:000360510800006
ER
PT J
AU Thompson, DR
Gao, BC
Green, RO
Roberts, DA
Dennison, PE
Lundeen, SR
AF Thompson, David R.
Gao, Bo-Cai
Green, Robert O.
Roberts, Dar A.
Dennison, Philip E.
Lundeen, Sarah R.
TI Atmospheric correction for global mapping spectroscopy: ATREM advances
for the HyspIRI preparatory campaign
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Imaging spectroscopy; HyspIRI mission; Atmospheric correction
ID VEGETATION LIQUID WATER; AVIRIS DATA; IMAGING SPECTROSCOPY; SATELLITE
SIGNAL; SOLAR SPECTRUM; SIERRA-NEVADA; RETRIEVAL; ALGORITHM; ABSORPTION;
SNOWMELT
AB Orbital imaging spectrometers, such as the proposed Hyperspectral Infrared Imager (HyspIRI) mission, will provide global, multi-year Visible Shortwave Infrared (VSWIR) reflectance maps. Monitoring the Earth's surface at high spectral resolution will advance our understanding of changing ecosystems and land use. These applications depend on reliable correction of atmospheric scattering and absorption. The HyspIRI Preparatory Campaign is an airborne precursor mission comprised of multiple flights by the "classic" Airborne Visible Infrared Imaging Spectrometer (AVIRIS-C) over a wide geographic area. This article describes the atmospheric correction that we have implemented for the campaign. We first present the theoretical basis of our approach, which is grounded in the ATmospheric REMoval (ATREM) algorithm. We then describe new enhancements including retrieval of pressure altitude, which improves accuracy over widely varying topography, and joint retrieval of optical absorption for three phases of water (vapor, liquid, and ice), which improves accuracy over vegetated areas. Reflectance is validated using ground spectra acquired across a wide range of targets and elevations. Finally, we use the algorithm to map vapor, liquid, and ice phases of water over 6 months across a 14,000 km(2) region of California. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Thompson, David R.; Green, Robert O.; Lundeen, Sarah R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gao, Bo-Cai] Naval Res Lab, Washington, DC USA.
[Roberts, Dar A.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA.
[Dennison, Philip E.] Univ Utah, Salt Lake City, UT USA.
RP Thompson, DR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 158-242, Pasadena, CA 91109 USA.
EM david.r.thompson@jpl.nasa.gov
OI Dennison, Philip/0000-0002-0241-1917
FU NASA [NNX12AP08G]; U.S. Government sponsorship [NAS7-1260]
FX We acknowledge the invaluable insight and counsel of HyspIRI Preparatory
Campaign investigators. We thank Ian McCubbin whose expertise and work
made the HyspIRI Preparatory Campaign possible. We also thank Brian Bue
and the members of the AVIRIS-C flight and data processing team,
including Scott Nolte, Mark Helmlinger, and Yasha Mouradi. We are
grateful to Susan Meerdink and Erin Wetherley for assistance and
locating calibration targets, collecting spectra and processing them.
The HyspIRI Preparatory Campaign is conducted under the oversight of the
NASA Earth Science Division. We are grateful for the continued support
of NASA Earth and climate scientists and particularly Woody Turner and
Diane Wickland. Support for this research was provided by NASA grant
#NNX12AP08G. A portion of this research was performed at the Jet
Propulsion Laboratory, California Institute of Technology. Copyright
2014. All Rights Reserved. U.S. Government sponsorship acknowledged
under NAS7-1260.
NR 41
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 15
PY 2015
VL 167
SI SI
BP 64
EP 77
DI 10.1016/j.rse.2015.02.010
PG 14
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CQ3OB
UT WOS:000360510800007
ER
PT J
AU Roberts, DA
Dennison, PE
Roth, KL
Dudley, K
Hulley, G
AF Roberts, Dar A.
Dennison, Philip E.
Roth, Keely L.
Dudley, Kenneth
Hulley, Glynn
TI Relationships between dominant plant species, fractional cover and Land
Surface Temperature in a Mediterranean ecosystem
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE HyspIRI; AVIRIS; MASTER; Mediterranean ecosystems; Multiple Endmember
Spectral Mixture Analysis Classification; Land Surface Temperature;
Spectroscopy
ID SPECTRAL MIXTURE ANALYSIS; IMAGING SPECTROMETER DATA; LEAF
OPTICAL-PROPERTIES; ENDMEMBER SELECTION; CANOPY NITROGEN; SPECTROSCOPIC
DETERMINATION; ABSORPTION FEATURES; CHAPARRAL SHRUBS; WATER-CONTENT;
FOREST
AB The Hyperspectral Infrared Imager (HyspIRI) is a proposed satellite mission that combines a 60 m spatial resolution Visible-Shortwave Infrared (VSWIR) imaging spectrometer and a 60 m multispectral thermal infrared (TIR) scanner. HyspIRI would combine the established capability of a VSWIR sensor to discriminate plant species and estimate accurate cover fractions with improved Land Surface Temperatures (LST) retrieved from the TIR sensor. We evaluate potential synergies between Airborne Visible/Infrared Imaging Spectrometer (AVIRIS) maps of dominant plant species and mixed species assemblages, fractional cover, and MODIS/ASTER Airborne Simulator (MASTER) LST utilizing multiple flight lines acquired in July 2011 in the Santa Barbara, California area. Species composition and green vegetation (GV), non-photosynthetic vegetation (NPV), impervious, and soil cover fractions were mapped using Multiple Endmember Spectral Mixture Analysis with a spectral library derived from 7.5 m imagery. Temperature-Emissivity Separation (TES) was accomplished using the MASTER TES algorithm. Pixel-based accuracy exceeded 50% for 23 species and land cover classes and approached 75% based on pixel majority in reference polygons. An inverse relationship was observed between CV fractions and LST. This relationship varied by dominant plant species/vegetation class, generating unique LST GV clusters. We hypothesize clustering is a product of environmental controls on species distributions, such as slope, aspect, and elevation as well as species-level differences in canopy structure, rooting depth, water use efficiency, and available soil moisture, suggesting that relationships between LST and plant species will vary seasonally. The potential of HyspIRI as a means of providing these seasonal relationships is discussed. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Roberts, Dar A.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
[Dennison, Philip E.; Dudley, Kenneth] Univ Utah, Dept Geog, Salt Lake City, UT 84112 USA.
[Roth, Keely L.] Univ Calif Davis, Dept Land, Air, Water Resources, Davis, CA 95616 USA.
[Hulley, Glynn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Roberts, DA (reprint author), Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
EM dar@geog.ucsb.edu
OI Dennison, Philip/0000-0002-0241-1917; Dudley,
Kenneth/0000-0003-3594-0724
FU NASA [NNX11AE44G, NNX12AP08G]
FX We wish to thank the Jet Propulsion Laboratory for providing
radiometrically calibrated, orthorectified AVIRIS and MASTER data. This
research was supported in part by NASA Grants NNX11AE44G, Evaluation of
Synergies between VNIR-SWIR and TIR Imagery in a Mediterranean-climate
ecosystem and NNX12AP08G, HyspIRI discrimination of plant species and
functional types along a strong environmental-temperature gradient. A
portion of this work was carried out at the Jet Propulsion
Laboratory/California Institute of Technology, Pasadena, California,
under contract with the National Aeronautics and Space Administration.
NR 78
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 15
PY 2015
VL 167
SI SI
BP 152
EP 167
DI 10.1016/j.rse.2015.01.026
PG 16
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CQ3OB
UT WOS:000360510800014
ER
PT J
AU Kudela, RM
Palacios, SL
Austerberry, DC
Accorsi, EK
Guild, LS
Torres-Perez, J
AF Kudela, Raphael M.
Palacios, Sherry L.
Austerberry, David C.
Accorsi, Emma K.
Guild, Liane S.
Torres-Perez, Juan
TI Application of hyperspectral remote sensing to cyanobacterial blooms in
inland waters
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Remote sensing; Inland waters; Phycocyanin; Cyanobacteria; Harmful algal
bloom; Califomia
ID SAN-FRANCISCO ESTUARY; MICROCYSTIS-AERUGINOSA; CLIMATE-CHANGE; MONTEREY
BAY; LAKE-ERIE; PHYTOPLANKTON; PHYCOCYANIN; CALIFORNIA; COASTAL;
TOXICITY
AB Cyanobacterial blooms are increasingly posing a severe threat to inland waters, particularly at the land-sea interface where toxins can be transported downstream with subsequent impacts to both terrestrial and marine organisms. These blooms are relatively easy to detect optically because of the surface concentration of cells, the presence of phycocyanin pigments, and the elevated backscatter associated with cell size and the presence of gas vacuoles. Major challenges limiting the use of remote sensing have been, first, that many of these water bodies are small relative to the spatial resolution of ocean color satellites, and second, even with a bright algal target, the spectral resolution, signal-to-noise ratio, and repeat time for terrestrial satellites is often inadequate. The next generation of multispectral and hyperspectral sensors begin to address these issues with both increased spatial and spectral resolution. Weekly monitoring of Pinto Lake, California has demonstrated that this small water body provides an ideal testbed for development and application of algorithms applicable for legacy and next-generation sensors. Pinto Lake experiences seasonal nearly monospecific blooms with a pronounced species succession. Biomass (as chlorophyll) within Pinto Lake seasonally ranges from similar to 1 to 1000 mu g/L. Pinto Lake has been within the flight lines for several recent airborne missions, including the HyspIRI Preparatory Flight Campaign, and is often targeted for HICO acquisitions. Using these data we demonstrate that spectral-shape algorithms requiring minimal atmospheric correction can be used across a range of legacy sensors to detect cyanobacterial blooms and that, with the availability of high spectral resolution data and appropriate atmospheric correction, it is possible to separate the cyanobacterial genera Aphanizomenon and Microcystis. In California Aphanizomenon is typically non-toxic and blooms prior to toxin-producing Micro cystis, thus leading to the potential for an early warning system based on the identification of algal types. (C) 2015 The Authors. Published by Elsevier Inc.
C1 [Kudela, Raphael M.] Univ Calif Santa Cruz, Ocean Sci Dept, Santa Cruz, CA 95064 USA.
[Palacios, Sherry L.] NASA, Ames Res Ctr, ORAU, Moffett Field, CA 94035 USA.
[Austerberry, David C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Accorsi, Emma K.] Emory Univ, Appl Math & Comp Sci, Atlanta, GA 30322 USA.
[Guild, Liane S.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
[Torres-Perez, Juan] NASA, Ames Res Ctr, BAERI, Moffett Field, CA 94035 USA.
RP Kudela, RM (reprint author), Univ Calif Santa Cruz, Ocean Sci Dept, 1156 High St, Santa Cruz, CA 95064 USA.
EM kudela@ucsc.edu; sherry.l.palacios@nasa.gov; dauster@umich.edu;
emma.accorsi@gmail.com; liane.s.guild@nasa.gov;
juan.l.torresperez@nasa.gov
FU NASA Student Airborne Research Program; City of Watsonville, California
Sea Grant [NA100AR4170060]; State of California Water Resources Control
Board [07-120-250]; NASA through the HyspIRI Airborne Campaign
[NNX12AQ23G]; NASA ACE Preparatory Activities [NNX13AKO4G]; Silicon
Valley Initiatives, NASA Ames University Affiliated Research Center
(UARC)
FX The initial analysis for this study was sponsored by the NASA Student
Airborne Research Program. We thank all the participants and organizers,
particularly Dr. Emily Schaller and Mr. Rick Shetter. Funding for the
field monitoring effort was provided by the City of Watsonville,
California Sea Grant award NA100AR4170060 and State of California Water
Resources Control Board contract 07-120-250. NASA support through the
HyspIRI Airborne Campaign provided support for data collection,
analysis, and synthesis through award NNX12AQ23G, and with field data
collection support from NASA ACE Preparatory Activities award NNX13AKO4G
and the Silicon Valley Initiatives, part of the NASA Ames University
Affiliated Research Center (UARC). The manuscript was greatly improved
with the comments provided by two anonymous reviewers and Professor Dar
Roberts (Guest Editor).
NR 60
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 15
PY 2015
VL 167
SI SI
BP 196
EP 205
DI 10.1016/j.rse.2015.01.025
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CQ3OB
UT WOS:000360510800017
ER
PT J
AU Palacios, SL
Kudela, RM
Guild, LS
Negrey, KH
Torres-Perez, J
Broughton, J
AF Palacios, Sherry L.
Kudela, Raphael M.
Guild, Liane S.
Negrey, Kendra H.
Torres-Perez, Juan
Broughton, Jennifer
TI Remote sensing of phytoplankton functional types in the coastal ocean
from the HyspIRI Preparatory Flight Campaign
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE HyspIRI; Biodiversity; Phytoplankton functional type; Harmful algal
bloom; Water quality; Atmospheric correction; PHYDOTax
ID ATMOSPHERIC CORRECTION; MONTEREY BAY; HYPERSPECTRAL IMAGER; COLOR
IMAGERY; CALIFORNIA; ALGORITHM; AIRBORNE; BLOOM; SEA; CHLOROPHYLL
AB The 2013-2015 Hyperspectral Infrared Imager (HyspIRI) Preparatory Flight Campaign, using the Airborne Visible/Infrared Imaging Spectrometer (AVIRIS) and MODIS/ASTER Airborne Simulator (MASTER), seeks to demonstrate appropriate sensor signal, spatial and spectral resolution, and orbital pass geometry for a global mission to reveal ecological and climatic gradients expressed in the selected California, USA study area. One of the awarded projects focused on the flight transects covering the coastal ocean to demonstrate that the AVIRIS data can be used to infer phytoplankton functional types at the land-sea interface. Specifically, this project directly assesses whether HyspIRI can provide adequate signal in the complex aquatic environment of the coastal zone to address questions of algal bloom dynamics, water quality, transient responses to human disturbance, river runoff, and red tides. Phytoplankton functional type (PFT), or biodiversity, can be determined from ocean color using the Phytoplankton Detection with Optics (PHYDOTax) algorithm and this information can be used to detect and monitor for harmful algal blooms. PHYDOTax is sensitive to spectral shape and accurate retrievals of ocean color across the visible spectral range is needed. The specific goal of this paper is to address the challenges of sensor capabilities and atmospheric correction in coastal environments by assessing two atmospheric correction methods using AVIRIS data for the retrieval of ocean color for use in derived products of chlorophyll-a and phytoplankton functional type. The atmospheric correction algorithms Atmospheric Removal (ATREM) and Tafkaa were applied to AVIRIS imagery of Monterey Bay, CA collected on 10 April 2013 and 31 October 2013. Data products from the imagery were compared with shipboard measurements including chlorophyll-a from whole-water samples and phytoplanlcton community structure estimated from diagnostic pigment markers using CHEMical TAXonomy (CHEMTAX). Using ATREM and Tafkaa and a selected set of input parameters for the scenes, we were unable to produce accurate retrievals of ocean color for the determination of chlorophyll-a and phytoplanlcton diversity. A modified ATREM correction produced science-quality data in which chlorophyll-a was accurately estimated using the Ocean Color 3 (00) chlorophyll-a algorithm, but biodiversity using PHYDOTax was not accurately estimated. Improvements in sensor calibration, sensitivity, and atmospheric correction of the HyspIRI imagery data set is needed in order to adequately estimate biogeochemically meaningful data products for the ocean such as chlorophyll-a, inherent optical properties, or PFfs. The HyspIRI Science Team is seeking improvements so the HyspIRI Airborne Campaign data set can be used for algorithm development to understand biodiversity and ecosystem function of coastal habitats that are facing increasing threats of human impact and climate change. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Palacios, Sherry L.] NASA, Ames Res Ctr, Oak Ridge Affiliated Univ, Moffett Field, CA 94035 USA.
[Kudela, Raphael M.; Negrey, Kendra H.; Broughton, Jennifer] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Guild, Liane S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Torres-Perez, Juan] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
RP Palacios, SL (reprint author), NASA, Ames Res Ctr, Oak Ridge Affiliated Univ, Moffett Field, CA 94035 USA.
EM sherry.l.palacios@nasa.gov; kudela@ucsc.edu; liane.s.guild@nasa.gov;
khyashi@ucsc.edu; juan.l.torresperez@nasa.gov; jbrought@ucsc.edu
FU NASA's Research Opportunities in Space and Earth Science (ROSES)
[NNH11ZDA001N]; NASA [RO 18729]
FX Funding to support this research was provided by NASA's Research
Opportunities in Space and Earth Science (ROSES-2011), NNH11ZDA001N,
Program Element A.26: HyspIRI Preparatory Airborne Activities and
Associated Science and Applications Research. Funding was provided to SP
from the NASA Postdoctoral Program Fellowship (RO 18729) administered by
the Oak Ridge Affiliated Universities (ORAU). SP wishes to thank B.C.
Gao, R.O. Green, D.R. Thompson, M. Peacock, I. McCubbin, and R. Pasetto
for technical assistance. We thank the editors of the HyspIRI special
issue for making this opportunity possible. We are very grateful to the
two anonymous reviewers who helped improve the manuscript with
thoughtful suggestions and guidance.
NR 54
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 15
PY 2015
VL 167
SI SI
BP 269
EP 280
DI 10.1016/j.rse.2015.05.014
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CQ3OB
UT WOS:000360510800023
ER
PT J
AU Baker, VR
Hamilton, CW
Burr, DM
Gulick, VC
Komatsu, G
Luo, W
Rice, JW
Rodriguez, JAP
AF Baker, Victor R.
Hamilton, Christopher W.
Burr, Devon M.
Gulick, Virginia C.
Komatsu, Goro
Luo, Wei
Rice, James W., Jr.
Rodriguez, J. A. P.
TI Fluvial geomorphology on Earth-like planetary surfaces: A review
SO GEOMORPHOLOGY
LA English
DT Review
DE Planetary geomorphology; Fluvial channels; Volcanic channels; Mars;
Venus; Titan
ID MARTIAN OUTFLOW CHANNELS; RECURRING SLOPE LINEAE; POTENTIAL FORMATION
MECHANISMS; CASSINI RADAR OBSERVATIONS; POLAR ICE-SHEET; EARLY MARS;
VALLES-MARINERIS; SEDIMENT TRANSPORT; ATHABASCA VALLES; LANDING SITE
AB Morphological evidence for ancient channelized flows (fluvial and fluvial-like landforms) exists on the surfaces of all of the inner planets and on some of the satellites of the Solar System. In some cases, the relevant fluid flows are related to a planetary evolution that involves the global cycling of a volatile component (water for Earth and Mars; methane for Saturn's moon Titan). In other cases, as on Mercury, Venus, Earth's moon, and Jupiter's moon lo, the flows were of highly fluid lava. The discovery, in 1972, of what are now known to be fluvial channels and valleys on Mars sparked a major controversy over the role of water in shaping the surface of that planet. The recognition of the fluvial character of these features has opened unresolved fundamental questions about the geological history of water on Mars, including the presence of an ancient ocean and the operation of a hydrological cycle during the earliest phases of planetary history. Other fundamental questions posed by fluvial and fluvial-like features on planetary bodies include the possible erosive action of large-scale outpourings of very fluid lavas, such as those that may have produced the remarkable canali forms on Venus; the ability of exotic fluids, such as methane, to create fluvial-like landforms, as observed on Saturn's moon, Titan; and the nature of sedimentation and erosion under different conditions of planetary surface gravity. Planetary fluvial geomorphology also illustrates fundamental epistemological and methodological issues, including the role of analogy in geomorphological/geological inquiry. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Baker, Victor R.; Hamilton, Christopher W.] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Burr, Devon M.] Univ Tennessee, Earth & Planetary Sci Dept, Knoxville, TN 37996 USA.
[Gulick, Virginia C.] SETI Inst, Mountain View, CA 94043 USA.
[Gulick, Virginia C.; Rodriguez, J. A. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Komatsu, Goro] Univ Annunzio, Int Res Sch Planetary Sci, I-65127 Pescara, Italy.
[Luo, Wei] No Illinois Univ, Dept Geog, De Kalb, IL 60115 USA.
[Rice, James W., Jr.; Rodriguez, J. A. P.] Planetary Sci Inst, Tucson, AZ 85719 USA.
RP Baker, VR (reprint author), Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
EM baker@email.arizona.edu
RI Komatsu, Goro/I-7822-2012
OI Komatsu, Goro/0000-0003-4155-108X
FU NASA Mars Fundamental Research Program grant [NNH10ZDA001N]; MRO HiRISE;
NASA Planetary Geology and Geophysics Program [NNX14AL54G]; Mars Data
Analysis Program [NNX14ANK77G]; NASA Mars Data Analysis Program; NASA
[NNX13AR11G, NNX08AM98G, NNX13AK65G]
FX We thank two anonymous reviewers for their comments on an earlier
version of this paper and Richard Marston for his detailed edits. VRB's
recent Mars studies were partly supported by a subcontract from a NASA
Mars Fundamental Research Program grant (#NNH10ZDA001N) to Michael
Mischna of the Jet Propulsion Laboratory. VCG was funded by as a MRO
HiRISE Co-Investigator. CWH acknowledges funding from NASA Planetary
Geology and Geophysics (Grant # NNX14AL54G) and Mars Data Analysis
(Grant # NNX14ANK77G) Programs. VRB and JR received funding trough the
NASA Mars Data Analysis Program. (grant # NNX13AR11G) WL was funded by
NASA grants # NNX08AM98G and # NNX13AK65G.
NR 431
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U2 76
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-555X
EI 1872-695X
J9 GEOMORPHOLOGY
JI Geomorphology
PD SEP 15
PY 2015
VL 245
BP 149
EP 182
DI 10.1016/j.geomorph.2015.05.002
PG 34
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA CQ3OF
UT WOS:000360511200012
ER
PT J
AU Bagheri, M
Spiers, GD
Frez, C
Forouhar, S
Aflatouni, F
AF Bagheri, Mahmood
Spiers, Gary D.
Frez, Clifford
Forouhar, Siamak
Aflatouni, Firooz
TI Linewidth Measurement of Distributed-Feedback Semiconductor Lasers
Operating Near 2.05 mu m
SO IEEE PHOTONICS TECHNOLOGY LETTERS
LA English
DT Article
DE Distributed-feedback lasers; fiber optics; mid-IR laser
ID CARBON-DIOXIDE; OUTPUT POWER; DFB LASER; WAVELENGTH; DIODE
AB The first unambiguous linewidth measurements are reported for fiber-pigtailed high-power distributed feedback (DFB) semiconductor lasers operating near 2.05 mu m wavelength range. The DFB lasers are packaged inside standard 14-pin butterfly package with polarization-maintaining output fiber and an integrated optical isolator. The Schawlow-Townes linewidth was measured using the coherent frequency-discriminator technique with a fiber Mach-Zehnder interferometer and the total linewidth was characterized using a heterodyne setup. Our measurements indicate less than 100 KHz Schawlow-Townes linewidth and a total linewidth of less than 200 KHz over 50 ms measurement time.
C1 [Bagheri, Mahmood; Spiers, Gary D.; Frez, Clifford; Forouhar, Siamak] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Aflatouni, Firooz] Univ Penn, Dept Elect & Syst Engn, Philadelphia, PA 19104 USA.
RP Bagheri, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mahmood.bagheri@jpl.nasa.gov; gary.d.spiers@jpl.nasa.gov;
clifford.f.frez@jpl.nasa.gov; siamak.forouhar@jpl.nasa.gov;
firooz@seas.upenn.edu
FU Advanced Component Technology (ACT) program of the National Aeronautics
and Space Administration's (NASA) Earth and Science Technology Office
(ESTO)
FX This work was supported under the Advanced Component Technology (ACT)
program of the National Aeronautics and Space Administration's (NASA)
Earth and Science Technology Office (ESTO).
NR 22
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U2 11
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1041-1135
EI 1941-0174
J9 IEEE PHOTONIC TECH L
JI IEEE Photonics Technol. Lett.
PD SEP 15
PY 2015
VL 27
IS 18
BP 1934
EP 1937
DI 10.1109/LPT.2015.2447286
PG 4
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA CQ1RA
UT WOS:000360375000011
ER
PT J
AU Guzewich, SD
Toigo, AD
Kulowski, L
Wang, HQ
AF Guzewich, Scott D.
Toigo, Anthony D.
Kulowski, Laura
Wang, Huiqun
TI Mars Orbiter Camera climatology of textured dust storms
SO ICARUS
LA English
DT Article
DE Mars, atmosphere; Atmospheres, dynamics; Meteorology
ID GENERAL-CIRCULATION MODEL; MARTIAN ATMOSPHERE; GLOBAL SURVEYOR;
INTERANNUAL VARIABILITY; NORTHERN-HEMISPHERE; POLAR-CAP; EVOLUTION;
SURFACE; CLOUDS; IMPACT
AB We report the climatology of "textured dust storms", those dust storms that have visible structure on their cloud tops that are indicative of active dust lifting, as observed in Mars Daily Global Maps produced from Mars Orbiter Camera wide-angle images. Textured dust storms predominantly occur in the equinox seasons while both solstice periods experience a planet-wide "pause" in textured dust storm activity. These pauses correspond to concurrent decreases in global atmospheric dust opacity. Textured dust storms most frequently occur in Acidalia Planitia, Chryse Planitia, Arcadia Planitia, and Hellas basin. To examine the nature of the link between textured dust storms and atmospheric dust opacity, we compare the textured dust storm climatology with a record of atmospheric dust opacity and find a peak global correlation coefficient of approximately 0.5 with a lag of 20-40 degrees in solar longitude in the opacity compared to the solar climatology. This implies that textured dust storms observed at 1400 local time by MOC are responsible for a large fraction of atmospheric dust opacity and that other mechanisms (e.g., dust devil lifting or storm-scale lifting not observed in this study) may supply a comparable amount of dust. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Guzewich, Scott D.] NASA, Goddard Space Flight Ctr, CRESST Univ Space Res Assoc, Greenbelt, MD 20771 USA.
[Toigo, Anthony D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Kulowski, Laura] Brown Univ, Providence, RI 02912 USA.
[Wang, Huiqun] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Guzewich, SD (reprint author), NASA, Goddard Space Flight Ctr, CRESST Univ Space Res Assoc, 8800 Greenbelt Rd,Code 693, Greenbelt, MD 20771 USA.
OI Guzewich, Scott/0000-0003-1149-7385
FU NASA [NNX13AK80G]
FX Dr. Guzewich was supported by a NASA Postdoctoral Fellowship. This work
was supported by the NASA Mars Data Analysis Program, Grant NNX13AK80G.
MarsWRF simulations were conducted on the NASA Pleiades Advanced
Supercomputer system. We thank Andrew Ingersoll and Richard Zurek for
their helpful reviews, which have greatly improved this paper.
NR 32
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U1 1
U2 14
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 15
PY 2015
VL 258
BP 1
EP 13
DI 10.1016/j.icarus.2015.06.023
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CO3XT
UT WOS:000359095300001
ER
PT J
AU Farnocchia, D
Chesley, SR
Micheli, M
AF Farnocchia, D.
Chesley, S. R.
Micheli, M.
TI Systematic ranging and late warning asteroid impacts
SO ICARUS
LA English
DT Article
DE Asteroids; Asteroids, dynamics; Astrometry; Near-Earth objects; Orbit
determination
ID NEAR-EARTH OBJECTS; ORBIT DETERMINATION; 2008 TC3; HAYABUSA
AB We describe systematic ranging, an orbit determination technique suitable to assess the near-term Earth impact hazard posed by newly discovered asteroids. For these late warning cases, the time interval covered by the observations is generally short, perhaps a few hours or even less, which leads to severe degeneracies in the orbit estimation process. The systematic ranging approach gets around these degeneracies by performing a raster scan in the poorly-constrained space of topocentric range and range rate, while the plane of sky position and motion are directly tied to the recorded observations. This scan allows us to identify regions corresponding to collision solutions, as well as potential impact times and locations. From the probability distribution of the observation errors, we obtain a probability distribution in the orbital space and then estimate the probability of an Earth impact. We show how this technique is effective for a number of examples, including 2008 TC3 and 2014 AA, the only two asteroids to date discovered prior to impact. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Farnocchia, D.; Chesley, S. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Micheli, M.] ESA NEO Coordinat Ctr, I-00044 Frascati, RM, Italy.
[Micheli, M.] SpaceDyS Srl, I-56023 Cascina, PI, Italy.
[Micheli, M.] INAF IAPS, I-00133 Rome, RM, Italy.
RP Farnocchia, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Davide.Farnocchia@jpl.nasa.gov
OI Micheli, Marco/0000-0001-7895-8209
NR 38
TC 4
Z9 4
U1 1
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 15
PY 2015
VL 258
BP 18
EP 27
DI 10.1016/j.icarus.2015.05.032
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CO3XT
UT WOS:000359095300003
ER
PT J
AU Koren, SC
Wright, EL
Mainzer, A
AF Koren, Seth C.
Wright, Edward L.
Mainzer, A.
TI Characterizing asteroids multiply-observed at infrared wavelengths
SO ICARUS
LA English
DT Article
DE Asteroids; Infrared observations; Asteroids, rotation
ID NEAR-EARTH ASTEROIDS; THERMAL-MODEL; THERMOPHYSICAL MODEL; RADIOMETRIC
METHOD; SURVEY-EXPLORER; NEOWISE; SHAPE; PERFORMANCE; METEORITES;
PLANETS
AB We report Markov chain Monte Carlo fits of the thermophysical model of Wright (Wright, E.L. [2007]. Astrophysics e-prints arXiv:astro-ph/0703058) to the fluxes of 10 asteroids which have been observed by both WISE and NEOWISE. This model is especially useful when one has observations of an asteroid at multiple epochs, as it takes advantage of the views of different local times and latitudes to determine the spin axis and the thermal parameter. Many of the asteroids NEOWISE observes will have already been imaged by WISE, so this proof of concept shows there is an opportunity to use a rotating cratered thermophysical model to determine surface thermal properties of a large number of asteroids. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Koren, Seth C.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Wright, Edward L.] UCLA Astron, Los Angeles, CA 90095 USA.
[Mainzer, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Koren, SC (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
EM korens@physics.upenn.edu; wright@astro.ucla.edu;
Amy.Mainzer@jpl.nasa.gov
FU NSF; Vagelos Challenge Award at the University of Pennsylvania; National
Aeronautics and Space Administration
FX This work was supported by the NSF and began during an REU program at
the University of California, Los Angeles.; SCK gratefully acknowledges
the support of the Vagelos Challenge Award at the University of
Pennsylvania.; This publication makes use of data products from the
Wide-field Infrared Survey Explorer, which is a joint project of the
University of California, Los Angeles, and the Jet Propulsion
Laboratory/California Institute of Technology, and NEOWISE, which is a
project of the Jet Propulsion Laboratory/California Institute of
Technology. WISE and NEOWISE are funded by the National Aeronautics and
Space Administration.
NR 36
TC 1
Z9 1
U1 0
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 15
PY 2015
VL 258
BP 82
EP 91
DI 10.1016/j.icarus.2015.06.014
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CO3XT
UT WOS:000359095300009
ER
PT J
AU Palomba, E
Longobardo, A
De Sanctis, MC
Zinzi, A
Ammannito, E
Marchi, S
Tosi, F
Zambon, F
Capria, MT
Russell, CT
Raymond, CA
Cloutis, EA
AF Palomba, Ernesto
Longobardo, Andrea
De Sanctis, Maria Cristina
Zinzi, Angelo
Ammannito, Eleonora
Marchi, Simone
Tosi, Federico
Zambon, Francesca
Capria, Maria Teresa
Russell, Christopher T.
Raymond, Carol A.
Cloutis, Edward A.
TI Detection of new olivine-rich locations on Vesta
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids, surfaces; Asteroids, composition; Mineralogy;
Spectroscopy
ID ASTEROID 4 VESTA; DARK MATERIAL; SPECTRAL PARAMETERS; BASALTIC
ASTEROIDS; DAWN MISSION; MAGMA OCEAN; PARENT BODY; GRAIN-SIZE;
DIOGENITES; EUCRITES
AB The discovery of olivine on Vesta's surface by the VIR imaging spectrometer onboard the Dawn space mission has forced us to reconsider our views of Vestan petrogenetic models. Olivines were expected to be present in the interior of Vesta: in the mantle of a vertically layered body as invoked by the magma ocean models, or at the base (or within) the mantle-crust boundary as proposed by fractionation models. Olivines have been detected by VIR-Dawn in two wide areas near Arruntia and Bellicia, regions located in the northern hemisphere. Interestingly, these olivine-rich terrains are far from the Rheasilvia and the more ancient Veneneia basins, which are expected to have excavated the crust down to reach the mantle. In this work we present our attempts to identify other undetected olivine rich areas on Vesta by using spectral parameters sensitive to olivine such as the Band Area Ratio (BAR) and other specific parameters created for the detection of olivines on Mars (forsterite, fayalite and a generic olivine index). As a preliminary step we calibrated these parameters by means of VIS-IR spectra of different RED meteorite samples: behaviors versus sample grain size and albedo were analyzed and discussed. We selected the BAR and the Forsterite Index as the best parameters that can be used on Vesta. A cross-correlation analysis has been applied in order to detect olivine signature on the VIR hyperspectral cubes. These detections have then been confirmed by an anti-correlation analysis between the BAR and one of the olivine parameters, independent of the first method applied.
In agreement with the recent discovery, Arruntia and Bellicia were found to be as the most olivine-rich areas, i.e. where the parameter values are strongest. In addition we detected 6 new regions, all but one located in the Vesta north hemisphere. This result confirms again that the old petrogenetic models cannot be straightforwardly applied to Vesta and should be reshaped in the view of these new detections. An alternative and very recent option can be represented by the model according to which surface "eruption" of material from the mantle, including olivine can reach the surface of Vesta. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Palomba, Ernesto; Longobardo, Andrea; De Sanctis, Maria Cristina; Tosi, Federico; Zambon, Francesca; Capria, Maria Teresa] INAF IAPS, I-00133 Rome, Italy.
[Zinzi, Angelo] INAF OAR, I-00040 Monte Porzio Catone, RM, Italy.
[Zinzi, Angelo] ESRIN, ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Ammannito, Eleonora; Russell, Christopher T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Marchi, Simone] Southwest Res Inst, Boulder, CO 80302 USA.
[Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cloutis, Edward A.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada.
RP Palomba, E (reprint author), INAF IAPS, Via Fosso del Cavaliere 100, I-00133 Rome, Italy.
OI ZINZI, Angelo/0000-0001-5263-5348; Palomba, Ernesto/0000-0002-9101-6774;
Tosi, Federico/0000-0003-4002-2434; Zambon,
Francesca/0000-0002-4190-6592
FU Dawn Science Team; Dawn Instrument Team; Dawn Operations Team; ASI;
NASA; Italian Space Agency - ASI
FX In Loving memory of my Dad, Gianni Palomba. The authors acknowledge the
support of the Dawn Science, Instrument, and Operations Teams. This work
was supported by ASI and NASA. A portion of this work was performed at
the NASA/JPL. The data used in this paper are available from the website
http://dawndata.igpp.ucla.edu. We warmly thank Robert Gaskell for
providing the Vesta shape model and Anton Ermakov for providing map of
the Vesta Bouguer anomaly. Thanks to Tom McCord (Bear Fight Institute)
and to another anonymous reviewer for suggestions and comments that
improved our manuscript. Diego Turrini (IAPS-INAF) is thanked for an
helpful discussion about exogenous origin of olivine. VIR is funded by
the Italian Space Agency - ASI and was developed under the leadership of
INAF-Istituto di Astrofisica e Planetologia Spaziali, Rome-Italy. The
instrument was built by Selex-Galileo, Florence-Italy.
NR 50
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U1 5
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 15
PY 2015
VL 258
BP 120
EP 134
DI 10.1016/j.icarus.2015.06.011
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CO3XT
UT WOS:000359095300012
ER
PT J
AU Loeffler, MJ
Hudson, RL
Chanoyer, NJ
Simon, AA
AF Loeffler, Mark J.
Hudson, Reggie L.
Chanoyer, Nancy J.
Simon, Amy A.
TI Giant-planet chemistry: Ammonium hydrosulfide (NH4SH), its IR spectra
and thermal and radiolytic stabilities
SO ICARUS
LA English
DT Article
DE Jupiter, atmosphere; Ices, IR spectroscopy; Geophysics; Atmospheres,
chemistry; Experimental techniques
ID INFRARED INTENSITY MEASUREMENTS; LIQUID-AMMONIA; THIN-FILMS; WATER ICE;
CLOUD STRUCTURE; IRRADIATION; JUPITER; SULFUR; IDENTIFICATION;
POLYSULFIDES
AB Here we present our recent studies of proton-irradiated and unirradiated ammonium hydrosulfide, NH4SH, a compound predicted to be an important tropospheric cloud component of Jupiter and other giant planets. We irradiated both crystalline and amorphous NH4SH at 10-160 K and used IR spectroscopy to observe and identify reaction products in the ice, specifically NH3 and long-chained sulfur-containing ions. Crystalline NH4SH was amorphized during irradiation at all temperatures studied with the rate being the fastest at the lowest temperatures. Irradiation of amorphous NH4SH at similar to 10-75 K showed that 60-80% of the NH4+ remained when equilibrium was reached, and that NH4SH destruction rates were relatively constant within this temperature range. Irradiations at higher temperatures produced different dose dependence and were accompanied by pressure outbursts that, in some cases, fractured the ice. The thermal stability of irradiated NH4SH was found to be greater than that of unirradiated NH4SH, suggesting that an irradiated giant-planet cloud precipitate can exist at temperatures and altitudes not previously considered. Published by Elsevier Inc.
C1 [Loeffler, Mark J.; Hudson, Reggie L.; Simon, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Chanoyer, Nancy J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
RP Loeffler, MJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Simon, Amy/C-8020-2012; Loeffler, Mark/C-9477-2012
OI Simon, Amy/0000-0003-4641-6186;
FU NASA's Planetary Atmospheres and Outer Planets Research programs
FX The support of NASA's Planetary Atmospheres and Outer Planets Research
programs is gratefully acknowledged. Carly Howett (SWRI, Boulder,
Colorado) is thanked for information on her NH4SH work and
for supplying spectral data. Steve Brown, Tom Ward, and Eugene
Gerashchenko, members of the NASA Goddard Radiation Effects Facility,
operated and maintained the Van de Graaff accelerator.
NR 58
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 15
PY 2015
VL 258
BP 181
EP 191
DI 10.1016/j.icarus.2015.06.015
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CO3XT
UT WOS:000359095300015
ER
PT J
AU Sylvestre, M
Guerlet, S
Fouchet, T
Spiga, A
Flasar, FM
Hesman, B
Bjoraker, GL
AF Sylvestre, M.
Guerlet, S.
Fouchet, T.
Spiga, A.
Flasar, F. M.
Hesman, B.
Bjoraker, G. L.
TI Seasonal changes in Saturn's stratosphere inferred from Cassini/CIRS
limb observations
SO ICARUS
LA English
DT Article
DE Saturn, atmosphere; Atmospheres, composition; Atmospheres, evolution;
Infrared observations
ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; LONG-TERM EVOLUTION; SPECTROSCOPIC
DATABASE; MERIDIONAL VARIATIONS; UPPER-ATMOSPHERE; GRAVITY-WAVES;
VOYAGER-IRIS; TEMPERATURES; JUPITER; ACETYLENE
AB We present temperature and hydrocarbons abundances (C2H6, C2H2, C3H8) retrieved from Cassini/CIRS limb spectra, acquired during northern spring in 2010 (L-s = 12 degrees) and 2012 (L-s = 31 degrees). We compare them to the previous limb measurements performed by Guerlet et al. (Guerlet, S. et al. [2009]. Icarus 203, 214-232) during northern winter. The latitudinal coverage (from 79 degrees N to 70 degrees S) and the sensitivity of our observations to a broad range of pressure levels (from 20 hPa to 0.003 hPa) allow us to probe the meridional and vertical structure of Saturn's stratosphere during northern spring. Our results show that in the northern hemisphere, the lower stratosphere (1 hPa) has experienced the strongest warming from northern winter to spring (11 +/-(11)(0.9) K), while the southern hemisphere exhibits weak variations of temperature at the same pressure level. We investigate the radiative contribution in the thermal seasonal evolution by comparing these results to the radiative-convective model of Guerlet et al. (Guerlet, S. et al. [2014]. Icarus 238, 110-124). We show that radiative heating and cooling by atmospheric minor constituents is not always sufficient to reproduce the measured variations of temperature (depending on the pressure level). The measurements of the hydrocarbons abundances and their comparison with the predictions of the 1D photochemical model of Moses and Greathouse (Moses, J.I., Greathouse, T.K. [2005]. J. Geophys. Res. (Planets) 110, 9007) give insights into large scale atmospheric dynamics. At 1 hPa, C2H6, C2H2, and C3H8 abundances are remarkably constant from northern winter to spring. At the same pressure level, C2H6 and C3H8 exhibit homogeneous meridional distributions unpredicted by this photochemical model, unlike C2H2. This is consistent with the existence of a meridional circulation at 1 hPa, as suggested by previous studies. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Sylvestre, M.; Fouchet, T.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, F-92195 Meudon, France.
[Sylvestre, M.; Guerlet, S.; Spiga, A.] CNRS, LMD, IPSL, UMR 8539, F-75005 Paris, France.
[Sylvestre, M.; Guerlet, S.; Fouchet, T.; Spiga, A.] Univ Paris 06, Univ Sorbonne, UMR 8109, F-75005 Paris, France.
[Flasar, F. M.; Bjoraker, G. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hesman, B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Sylvestre, M (reprint author), Observ Paris, LESIA, 5 Pl Jules Janssen, F-92195 Meudon, France.
EM melody.sylvestre@obspm.fr
RI Spiga, Aymeric/O-4858-2014; Flasar, F Michael/C-8509-2012; Fouchet,
Thierry/C-6374-2017
OI Spiga, Aymeric/0000-0002-6776-6268; Fouchet, Thierry/0000-0001-9040-8285
FU Emergence Program of UPMC; French ANR [ANR-12-PDOC-0013]; Institut
Universitaire de France
FX M. Sylvestre, A. Spiga and T. Fouchet acknowledge funding by the
Emergence Program of UPMC. S. Guerlet acknowledges funding by the French
ANR under Grant agreement ANR-12-PDOC-0013. Part of this work was also
funded by the Institut Universitaire de France. We also thank D. Strobel
for his suggestions about the heating processes of the upper
stratosphere, the Cassini/CIRS team for their calibration and planning
of the data, and the reviewers for their constructive comments on this
paper.
NR 46
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 15
PY 2015
VL 258
BP 224
EP 238
DI 10.1016/j.icarus.2015.05.025
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CO3XT
UT WOS:000359095300017
ER
PT J
AU Batalha, N
Domagal-Goldman, SD
Ramirez, R
Kasting, JF
AF Batalha, Natasha
Domagal-Goldman, Shawn D.
Ramirez, Ramses
Kasting, James F.
TI Testing the early Mars H-2-CO2 greenhouse hypothesis with a 1-D
photochemical model
SO ICARUS
LA English
DT Article
DE Mars; Photochemistry; Volcanism
ID EARTHS EARLY ATMOSPHERE; EARLY MARTIAN CLIMATE; IRON-FORMATIONS;
EVOLUTION; CO2; MANTLE; CONSTRAINTS; CHEMISTRY; NITROGEN; PLANETS
AB A recent study by Ramirez et al. (Ramirez, R.M. et al. [2014]. Nat. Geosci. 7(1), 59-63. (accessed 16.09.14)) demonstrated that an atmosphere with 1.3-4 bar of CO2 and H2O, in addition to 5-20% H-2, could have raised the mean annual and global surface temperature of early Mars above the freezing point of water. Such warm temperatures appear necessary to generate the rainfall (or snowfall) amounts required to carve the ancient martian valleys. Here, we use our best estimates for early martian outgassing rates, along with a 1-D photochemical model, to assess the conversion efficiency of CO, CH4, and H2S to CO2, SO2, and H-2. Our outgassing estimates assume that Mars was actively recycling volatiles between its crust and interior, as Earth does today. H-2 production from serpentinization and deposition of banded iron-formations is also considered. Under these assumptions, maintaining an H-2 concentration of similar to 1-2% by volume is achievable, but reaching 5% H-2 requires additional H-2 sources or a slowing of the hydrogen escape rate below the diffusion limit. If the early martian atmosphere was indeed H-2-rich, we might be able to see evidence of this in the rock record. The hypothesis proposed here is consistent with new data from the Curiosity Rover, which show evidence for a long-lived lake in Gale Crater near Mt. Sharp. It is also consistent with measured oxygen fugacities of martian meteorites, which show evidence for progressive mantle oxidation over time. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Batalha, Natasha] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Batalha, Natasha; Kasting, James F.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Batalha, Natasha; Domagal-Goldman, Shawn D.; Kasting, James F.] NASA Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA.
[Domagal-Goldman, Shawn D.] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA.
[Ramirez, Ramses] Cornell Univ, Carl Sagan Inst, Ithaca, NY 14850 USA.
[Ramirez, Ramses] Cornell Univ, Dept Astron, Ithaca, NY 14850 USA.
[Ramirez, Ramses] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14850 USA.
[Kasting, James F.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
RP Batalha, N (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM neb149@psu.edu
FU National Science Foundation [DGE1255832]; NASA's Exobiology and
Astrobiology programs; Simon's Foundation [SCOL 290357]; Carl Sagan
Institute
FX This material is based upon work supported by the National Science
Foundation under Grant No. DGE1255832 to N. Batalha. Any opinions,
findings, and conclusions or recommendations expressed in this material
are those of the author(s) and do not necessarily reflect the views of
the National Science Foundation. JFK acknowledges support from NASA's
Exobiology and Astrobiology programs. R.R. acknowledges support from the
Simon's Foundation (SCOL 290357, L.K.) and the Carl Sagan Institute.
NR 85
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 15
PY 2015
VL 258
BP 337
EP 349
DI 10.1016/j.icarus.2015.06.016
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CO3XT
UT WOS:000359095300023
ER
PT J
AU Roush, TL
Bishop, JL
Brown, AJ
Blake, DF
Bristow, TF
AF Roush, Ted L.
Bishop, Janice L.
Brown, Adrian J.
Blake, David F.
Bristow, Thomas F.
TI Laboratory reflectance spectra of clay minerals mixed with Mars analog
materials: Toward enabling quantitative clay abundances from Mars
spectra
SO ICARUS
LA English
DT Article
DE Mars; Mars, surface; Mineralogy
ID SOCIETY SOURCE CLAYS; MAWRTH VALLIS; BASE-LINE; SNC METEORITES;
SPECTROSCOPY; MIXTURES; MONTMORILLONITE; PHYLLOSILICATES; INSTRUMENT;
PALAGONITE
AB Quantitative estimates of clay minerals on the martian surface, via remote sensing observations, provide constraints on activity, timing, duration, and extent of aqueous processes and the geochemical environment in martian history. We describe an analytical study to begin enabling quantitative estimates of phyllosilicates when mixed with martian analog materials. We characterize the chemistry, mineralogy, particle size distribution, and reflectance spectra of the end-member materials: saponite, montmorillonite, pyroxene, and palagonitic soil. Reflectance spectra were obtained for physical mixtures of saponite and montmorillonite with pyroxene, and saponite with palagonitic soil. We analyzed the diagnostic phyllosilicate spectral signatures in the 2.2-2.4 mu m wavelength region in detail for the mixtures. This involved fitting the observed similar to 2.3 or similar to 2.2 mu m band depth, associated with the presence of saponite and montmorillonite, respectively, as a function of the abundance of these materials in the mixtures. Based upon the band depth of the spectral features we find that 3-5 wt.% of the clay minerals in the mixture with pyroxene can be recognized and at 25 wt.% their presence is indisputable in the mixtures. When the saponite is mixed with the lower albedo palagonitic soil, its presence is clearly distinguishable via the 1.4 and 2.3 pin features at 25 wt.% abundance. These relationships, between abundance and band depth, provide an ability to quantitatively address the amount of these materials in mixtures. The trends described here provide guidance for estimating the presence of phyllosilicates in matrices on the martian surface. Published by Elsevier Inc.
C1 [Roush, Ted L.; Bishop, Janice L.; Brown, Adrian J.; Blake, David F.; Bristow, Thomas F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bishop, Janice L.; Brown, Adrian J.] SETI Inst, Moffett Field, CA 94035 USA.
RP Roush, TL (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.
EM Ted.L.Roush@nasa.gov
FU NASA's Mars Fundamental Research Program
FX We are extremely grateful to the support from NASA's Mars Fundamental
Research Program. We thank Kathryn Stack and an anonymous reviewer for
their comments that helped in improving the manuscript.
NR 75
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 15
PY 2015
VL 258
BP 454
EP 466
DI 10.1016/j.icarus.2015.06.035
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CO3XT
UT WOS:000359095300031
ER
PT J
AU Plante, I
Devroye, L
AF Plante, Ianik
Devroye, Luc
TI On the Green's function of the partially diffusion-controlled reversible
ABCD reaction for radiation chemistry codes
SO JOURNAL OF COMPUTATIONAL PHYSICS
LA English
DT Article
DE Theory; Modeling; Computer simulation; Sampling algorithm; Monte Carlo
simulations; Green's functions of the diffusion equation; Chemical
reactions; Radiation chemistry
ID MONTE-CARLO-SIMULATION; BIMOLECULAR REACTIONS; LIQUID WATER;
3-DIMENSIONAL SIMULATIONS; GEMINATE RECOMBINATION; FRICKE DOSIMETER;
ONE-DIMENSION; RADIOLYSIS; KINETICS; ELECTRON
AB Several computer codes simulating chemical reactions in particles systems are based on the Green's functions of the diffusion equation (GFDE). Indeed, many types of chemical systems have been simulated using the exact GFDE, which has also become the gold standard for validating other theoretical models. In this work, a simulation algorithm is presented to sample the interparticle distance for partially diffusion-controlled reversible ABCD reaction. This algorithm is considered exact for 2-particles systems, is faster than conventional look-up tables and uses only a few kilobytes of memory. The simulation results obtained with this method are compared with those obtained with the independent reaction times (IRT) method. This work is part of our effort in developing models to understand the role of chemical reactions in the radiation effects on cells and tissues and may eventually be included in event-based models of space radiation risks. However, as many reactions are of this type in biological systems, this algorithm might play a pivotal role in future simulation programs not only in radiation chemistry, but also in the simulation of biochemical networks in time and space as well. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Plante, Ianik] Wyle Sci Technol & Engn, Houston, TX 77058 USA.
[Devroye, Luc] McGill Univ, Sch Comp Sci, Montreal H3A 0E9, PQ, Canada.
RP Plante, I (reprint author), NASA Johnson Space Ctr, Bldg 37,Mail Code SK,2101 NASA Pkwy, Houston, TX 77058 USA.
EM ianik.plante-1@nasa.gov; lucdevroye@gmail.com
FU National Aeronautics and Space Administration (NASA) [NAS9-02078]
FX We would like to thank the reviewers for their careful review and
comments. This work was supported by the National Aeronautics and Space
Administration (NASA) Bioastronautics Contract NAS9-02078.
NR 34
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0021-9991
EI 1090-2716
J9 J COMPUT PHYS
JI J. Comput. Phys.
PD SEP 15
PY 2015
VL 297
BP 515
EP 529
DI 10.1016/j.jcp.2015.05.007
PG 15
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA CM2WB
UT WOS:000357541900029
ER
PT J
AU Trail, M
Tsimpidi, AP
Liu, P
Tsigaridis, K
Hu, Y
Nenes, A
Stone, B
Russell, AG
AF Trail, M.
Tsimpidi, A. P.
Liu, P.
Tsigaridis, K.
Hu, Y.
Nenes, A.
Stone, B.
Russell, A. G.
TI Reforestation and crop land conversion impacts on future regional air
quality in the Southeastern US
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE LULCC; Climate change; Air quality; Reforestation
ID CMAQ MODELING SYSTEM; CLIMATE-CHANGE; UNITED-STATES; ATMOSPHERIC
CHEMISTRY; EMISSIONS; OZONE; SENSITIVITIES; SCENARIOS; WEATHER; VERSION
AB Land in the southeastern U.S. is expected to change, e.g., given the potential demand to develop forest-to-fuel technologies or, conversely, cropification of current forests to increase food production. Possible future PM2.5 and O-3 air quality for two land use/land cover change (LULCC) scenarios, reforestation and cropland conversion, are compared to a reference case scenario for the year 2050 using the Weather Research and Forecasting (WRF) and Community Multi-scale Air Quality (CMAQ) models. Changes in air quality driven by changes in climate, deposition and emissions relating to the LULCC are investigated. Reforestation in the Southeast tends to decrease the ambient O-3 mixing ratio while slightly increasing summertime PM2.5 in the Southeastern U.S. Results of a climate and deposition (CD) sensitivity simulation are provided for the two alternative LULCC scenarios to isolate the impact of changing climate and deposition on PM2.5 and O-3 air quality. The sensitivity results indicate that deposition and emissions changes associated with reforestation impact O-3 and PM2.5 concentrations as much as, and in most cases more than, changes in meteorology. Conversion of forest to cropland in the Southeast, on the other hand, tends to increase O-3 and increase PM2.5 year-round. Cropland conversion leads to increased NOx emissions and increases in the 4th highest maximum daily 8-h O-3 (MDA8) of the year by up to 10 ppb despite the tendency for increased deposition and decreased temperature to reduce the MDA8 mixing ratio. The results of this study show that O-3 and aerosol concentrations are sensitive to reforestation and cropland conversion in the Southeast and these land use changes should be considered in air quality management plans. Further, they show the sensitivity of such calculations to land cover properties. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Trail, M.; Tsimpidi, A. P.; Liu, P.; Hu, Y.; Russell, A. G.] Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA.
[Tsigaridis, K.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Tsigaridis, K.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Nenes, A.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Nenes, A.] Georgia Inst Technol, Sch Chem & Biomol Engn, Atlanta, GA 30332 USA.
[Stone, B.] Georgia Inst Technol, Sch City & Reg Planning, Atlanta, GA 30332 USA.
RP Trail, M (reprint author), Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA.
EM mcus2rail@gmail.com
RI Hu, Yongtao/H-7543-2016
OI Hu, Yongtao/0000-0002-5161-0592
FU US EPA [RD-83428101]; NASA
FX While this work was supported, in part, by grants from the US EPA
(RD-83428101) and NASA, reference herein to any specific commercial
products, process, or service by trade name, trademark, manufacturer, or
otherwise, does not necessarily constitute or imply their endorsement or
recommendation. The views and opinions of authors expressed herein are
those of the authors and do not necessarily state or reflect those of
the United States Government.
NR 48
TC 0
Z9 0
U1 1
U2 23
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
EI 1873-2240
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD SEP 15
PY 2015
VL 209
BP 78
EP 86
DI 10.1016/j.agrformet.2015.05.001
PG 9
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA CL7GX
UT WOS:000357141600008
ER
PT J
AU Balmer, BC
Ylitalo, GM
McGeorge, LE
Baugh, KA
Boyd, D
Mullin, KD
Rosel, PE
Sinclair, C
Wells, RS
Zolman, ES
Schwacke, LH
AF Balmer, Brian C.
Ylitalo, Gina M.
McGeorge, Lauren E.
Baugh, Keri A.
Boyd, Daryle
Mullin, Keith D.
Rosel, Patricia E.
Sinclair, Carrie
Wells, Randall S.
Zolman, Eric S.
Schwacke, Lori H.
TI Persistent organic pollutants (POPs) in blubber of common bottlenose
dolphins (Tursiops truncatus) along the northern Gulf of Mexico coast,
USA
SO SCIENCE OF THE TOTAL ENVIRONMENT
LA English
DT Article
DE Common bottlenose dolphin; Deepwater Horizon oil spill; Gulf of Mexico;
Persistent organic pollutants; Tursiops truncatus
ID MINK MUSTELA-VISON; C FUEL-OIL; POLYCHLORINATED BIPHENYL EXPOSURE;
SARASOTA BAY; ORGANOCHLORINE CONTAMINANTS; ATLANTIC COAST; LIFE-HISTORY;
HARBOR SEALS; FLORIDA; TRANSTHYRETIN
AB A number of studies were initiated in response to the Deepwater Horizon (DWH) oil spill to understand potential injuries to bottlenose dolphins (Tursiops truncatus) that inhabit the northern Gulf of Mexico (NGoM) estuarine waters. As part of these studies, remote biopsy skin and blubber samples were collected from dolphins at six field sites that received varying degrees of oiling: Barataria Bay (BB), Chandeleur Sound West (CSW), Chandeleur Sound East (CSE), Mississippi Sound South (MSS), Mississippi Sound North (MSN), and St. Joseph Bay (SJ). Blubber samples from 108 male dolphins were analyzed for persistent organic pollutant (POP) concentrations, as high levels of POPs have been previously reported in other southeastern U.S. dolphins and the potential contribution of these compounds to adverse health effects in NGoM dolphins must be considered. Dolphin blubber levels of summed POPs (Sigma POPs) did not differ significantly across sites (F-test, P = 0.9119) [mu g/g lipid; geometric mean and 95% CI]; CSW [65.9 (51.4-84.6)], SJ [74.1 (53.0-104)], MSN [74.3 (58.7-93.9)], BB [75.3 (56.4-101)], CSE [80.5 (57.8-112)], and MSS [82.5 (65.9-103)]. Overall, POP concentrations were in the lower half of the range compared to previously reported concentrations from other southeastern U.S. sites. Increased dolphin mortalities have been ongoing in the NGoM and have been suggested to be linked with the DWH oil spill. In addition, lung disease, impaired adrenal function, and serumbiochemical abnormalities have been reported in dolphins from BB, an area that was heavily oiled. The results of this study suggest that POPs are likely not a primary contributor to the poor health conditions and increased mortality observed in some populations of NGoM dolphins following the DWH oil spill. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Balmer, Brian C.; McGeorge, Lauren E.; Zolman, Eric S.; Schwacke, Lori H.] NOAA, NCCOS, Charleston, SC 29412 USA.
[Balmer, Brian C.; Wells, Randall S.] Mote Marine Lab, Chicago Zool Soc, Sarasota, FL 34236 USA.
[Ylitalo, Gina M.; Baugh, Keri A.; Boyd, Daryle] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA.
[Mullin, Keith D.; Sinclair, Carrie] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Pascagoula, MS 39567 USA.
[Rosel, Patricia E.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Lafayette, LA 70506 USA.
RP Balmer, BC (reprint author), NOAA, NCCOS, Hollings Marine Lab, 331 Ft Johnson Rd, Charleston, SC 29412 USA.
EM Brian.Balmer@noaa.gov
NR 47
TC 7
Z9 7
U1 2
U2 153
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0048-9697
EI 1879-1026
J9 SCI TOTAL ENVIRON
JI Sci. Total Environ.
PD SEP 15
PY 2015
VL 527
BP 306
EP 312
DI 10.1016/j.scitotenv.2015.05.016
PG 7
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA CK4WY
UT WOS:000356225300032
PM 25965044
ER
PT J
AU Behrangi, A
Nguyen, H
Lambrigtsen, B
Schreier, M
Dang, V
AF Behrangi, Ali
Hai Nguyen
Lambrigtsen, Bjorn
Schreier, Mathias
Dang, Van
TI Investigating the role of multi-spectral and near surface temperature
and humidity data to improve precipitation detection at high latitudes
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Precipitation; High latitude; Multi-spectral; Humidity; Temperature
ID SATELLITE INFRARED TECHNIQUE; CLOUD CLASSIFICATION-SYSTEM; ARTIFICIAL
NEURAL-NETWORKS; COMBINED PASSIVE MICROWAVE; CONTINENTAL UNITED-STATES;
RAINFALL ESTIMATION; GAUGE MEASUREMENTS; PROFILING RADAR; SOUNDING UNIT;
ALGORITHM
AB Accurate estimation of global precipitation is critical for the study of the earth in a changing climate. It is generally understood that instantaneous retrieval of precipitation using microwave sensors is more accurate in the tropics and mid latitudes, but the retrievals become difficult and uncertain at higher latitude and over frozen land. In the lack of reliable microwave-based precipitation estimates at high latitudes, retrievals from a single infrared band are commonly used as an alternative to fill the missing gaps. The present study shows that multi-spectral infrared, near-surface air temperature, and near-surface humidity data can add useful information to that obtained from a single infrared band and can significantly improve delineating precipitating from non-precipitating scenes, especially at higher latitudes over land. The role of surface air temperature and humidity is found to be more effective at higher latitudes, but multispectral data is effective across all latitudes. The study is performed using 4 years (2007-2010) of collocated multi-spectral data from the Moderate Resolution Imaging Spectroradiometer (MODIS), surface temperature and humidity data from the European Center for Medium Range Weather Forecast (ECMWF) analysis, and reference precipitation data from CloudSat, which can detect even very light precipitation within 80 degrees S-80 degrees N. (C) 2014 Published by Elsevier B.V.
C1 [Behrangi, Ali; Hai Nguyen; Lambrigtsen, Bjorn; Schreier, Mathias; Dang, Van] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 233-304, Pasadena, CA 91109 USA.
EM Ali.Behrangi@jpl.nasa.gov
FU National Aeronautics and Space Administration; NASA
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. The
study is partially supported by the NASA new investigator and the
Weather awards. Government sponsorship is acknowledged.
NR 77
TC 2
Z9 2
U1 1
U2 23
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD SEP 15
PY 2015
VL 163
SI SI
BP 2
EP 12
DI 10.1016/j.atmosres.2014.10.019
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CK4HE
UT WOS:000356184100002
ER
PT J
AU Ferraro, R
Beauchamp, J
Cecil, D
Heymsfield, G
AF Ferraro, Ralph
Beauchamp, James
Cecil, Daniel
Heymsfield, Gerald
TI A prototype hail detection algorithm and hail climatology developed with
the advanced microwave sounding unit (AMSU)
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Remote sensing; Passive microwave; Hail; Climatology; AMSU; MHS
ID LAND; RADIOMETRY; CONVECTION
AB In previous studies published in the open literature, a strong relationship between the occurrence of hail and the microwave brightness temperatures (primarily at 37 and 85 GHz) was documented. These studies were performed with the Nimbus-7 Scanning Multichannel Microwave Radiometer (SMMR), the Tropical Rainfall Measuring Mission (TRMM) Microwave Imager (TMI) and most recently, the Aqua Advanced Microwave Scanning Radiometer (AMSR-E) sensor. This led to climatologies of hail frequency from TMI and AMSR-E, however, limitations included geographical domain of the TMI sensor (35 S to 35 N) and the overpass time of the Aqua satellite (130 am/pm local time), both of which reduce an accurate mapping of hail events over the global domain and the full diurnal cycle. Nonetheless, these studies presented exciting, new applications for passive microwave sensors. NOAA and EUMETSAT have been operating the Advanced Microwave Sounding Unit (AMSU-A and -B) and the Microwave Humidity Sounder (MHS) on several operational satellites since 1998: NOAA-15 through NOAA-19; MetOp-A and -B. With multiple satellites in operation since 2000, the AMSU/MHS sensors provide near global coverage every 4 h, thus, offering a much larger time and temporal sampling than TRMM or AMSR-E. With similar observation frequencies near 30 and 85 GHz, one at 157 GHz, and additionally three at the 183 GHz water vapor band, the potential to detect strong convection associated with severe storms on a more comprehensive time and space scale exists.
In this study, we develop a prototype AMSU-based hail detection algorithm through the use of collocated satellite and surface hail reports over the continental US for a 10-year period (2000-2009). Compared with the surface observations, the algorithm detects approximately 40% of hail occurrences. The simple threshold algorithm is then used to generate a hail climatology based on all available AMSU observations during 2000-2011 that is stratified in several ways, including total hail occurrence by month (March through September), total annual, and over the diurnal cycle. Independent comparisons are made compared to similar data sets derived from other satellite, ground radar and surface reports. The algorithm was also applied to global land measurements for a single year and showed close agreement with other satellite based hail climatologies. Such a product could serve as a prototype for use with a future geostationary based microwave sensor such as NASA's proposed PATH mission. Published by Elsevier B.V.
C1 [Ferraro, Ralph] NOAA NESDIS, College Pk, MD 20740 USA.
[Ferraro, Ralph; Beauchamp, James] Univ Maryland, Cooperat Inst Climate & Satellites, College Pk, MD 20742 USA.
[Cecil, Daniel] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Heymsfield, Gerald] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ferraro, R (reprint author), NOAA NESDIS, 5825 Univ Res Court,Suite 4001, College Pk, MD 20740 USA.
EM Ralph.R.Ferraro@noaa.gov; vajim@essic.umd.edu; Daniel.J.Cecil@nasa.gov;
Gerald.M.Heymsfield@nasa.gov
RI Ferraro, Ralph/F-5587-2010;
OI Ferraro, Ralph/0000-0002-8393-7135; Heymsfield,
Gerald/0000-0001-6298-0233
NR 25
TC 5
Z9 5
U1 0
U2 17
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD SEP 15
PY 2015
VL 163
SI SI
BP 24
EP 35
DI 10.1016/j.atmosres.2014.08.010
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CK4HE
UT WOS:000356184100004
ER
PT J
AU Tang, L
Tian, YD
Yan, F
Habib, E
AF Tang, Ling
Tian, Yudong
Yan, Fang
Habib, Emad
TI An improved procedure for the validation of satellite-based
precipitation estimates
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Satellite-based precipitation estimates; Validation procedure; Additive
and multiplicative error model; Logarithmic transformation; Uncertainty
estimation
ID CONTINENTAL UNITED-STATES; PASSIVE MICROWAVE; SAMPLING ERROR;
INTERCOMPARISON PROJECT; RAINFALL AVERAGES; RADAR DATASET; GAUGE DATA;
RESOLUTION; PRODUCTS; MODEL
AB The objective of this study is to propose and test a new procedure to improve the validation of remote-sensing, high-resolution precipitation estimates. Our recent studies show that many conventional validation measures do not accurately capture the unique error characteristics in precipitation estimates to better inform both data producers and users. The proposed new validation procedure has two steps: 1) an error decomposition approach to separate the total retrieval error into three independent components: hit error, false precipitation and missed precipitation: and 2) the hit error is further analyzed based on a multiplicative error model. In the multiplicative error model, the error features are captured by three model parameters. In this way, the multiplicative error model separates systematic and random errors, leading to more accurate quantification of the uncertainties. The proposed procedure is used to quantitatively evaluate the recent two versions (Version 6 and 7) of TRMM's Multi-sensor Precipitation Analysis (TMPA) real-time and research product suite (3B42 and 3B42RT) for seven years (2005-2011) over the continental United States (CONUS). The gauge-based National Centers for Environmental Prediction (NCEP) Climate Prediction Center (CPC) near-real-time daily precipitation analysis is used as the reference. In addition, the radar-based NCEP Stage IV precipitation data are also model-fitted to verify the effectiveness of the multiplicative error model. The results show that winter total bias is dominated by the missed precipitation over the west coastal areas and the Rocky Mountains, and the false precipitation over large areas in Midwest. The summer total bias is largely coming from the hit bias in Central US. Meanwhile, the new version (V7) tends to produce more rainfall in the higher rain rates, which moderates the significant underestimation exhibited in the previous V6 products. Moreover, the error analysis from the multiplicative error model provides a clear and concise picture of the systematic and random errors, with both versions of 3B42RT have higher errors in varying degrees than their research (post-real-time) counterparts. The new V7 algorithm shows obvious improvements in reducing random errors in both winter and summer seasons, compared to its predecessors V6. Stage IV, as expected, surpasses the satellite-based datasets in all the metrics over CONUS. Based on the results, we recommend the new procedure be adopted for routine validation of satellite-based precipitation datasets, and we expect the procedure will work effectively for higher resolution data to be produced in the Global Precipitation Measurement (GPM) era. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Tang, Ling; Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Tang, Ling; Tian, Yudong] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Yan, Fang; Habib, Emad] Univ Louisiana Lafayette, Dept Civil Engn, Lafayette, LA 70504 USA.
RP Tang, L (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Code 617, Greenbelt, MD 20771 USA.
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 Climates Simulation. We appreciate the very helpful
suggestions from two anonymous reviewers.
NR 50
TC 11
Z9 12
U1 6
U2 53
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD SEP 15
PY 2015
VL 163
SI SI
BP 61
EP 73
DI 10.1016/j.atmosres.2014.12.016
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CK4HE
UT WOS:000356184100007
ER
PT J
AU Liu, Z
AF Liu, Zhong
TI Comparison of versions 6 and 7 3-hourly TRMM multi-satellite
precipitation analysis (TMPA) research products
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Precipitation; Comparison; TMPA; Satellite; Remote sensing
ID GLOBAL PRECIPITATION; PASSIVE MICROWAVE; ALGORITHM; SYSTEM;
VISUALIZATION; INFORMATION; VALIDATION; RESOLUTION; GIOVANNI; RAINFALL
AB This paper examines differences between Version 6 (V6) and Version 7 (V7) 3-hourly TRMM (Tropical Rainfall Measuring Mission) Multi-Satellite Precipitation Analysis (TMPA 3B42) research products in BA (June, July and August) and DJF (December, January and February) over a 13-year period from 1998 to 2010 on a global scale. Different surface types and rain regimes are considered in the comparison. The study finds that more rain events are found in V7 than those in V6 in both JJA and DJF, especially over oceans. Overall, both versions show a good agreement in moderate and heavy rain regimes. High Pearson's correlation coefficients are found in tropical rain band regions. Histograms of both versions are very similar; however higher frequencies of rain events are found in V7 in light rain regime, especially over oceans, than those in V6. For light rain, rainfall estimates in V6 are less than those in V7 over land and oceans in both seasons. For moderate rain, rainfall estimates in V6 are larger than those in V7 over land in most years. Over oceans, it is a mixed situation in which V6 > V7 for some years and V6 < V7 for the other years. For heavy rain, rainfall estimates in V6 are larger than those in V7 throughout all BA and DJF seasons for both land and oceans, which is also shown in a case study. Large variance in the individual differences is found in light rain and less in heavy rain. No apparent trends are observed. For light rain, all statistics support that there is an uncertainty issue in both versions. (C) 2015 The Author. Published by Elsevier B.V.
C1 [Liu, Zhong] George Mason Univ, Ctr Spatial Informat Sci & Syst, Fairfax, VA 22030 USA.
[Liu, Zhong] NASA, Goddard Space Flight Ctr, Goddard Earth Sci Data & Informat Serv Ctr, Greenbelt, MD 20771 USA.
RP Liu, Z (reprint author), George Mason Univ, Ctr Spatial Informat Sci & Syst, Fairfax, VA 22030 USA.
EM Zhong.Liu@nasa.gov
FU NASA [NNH10ZDA001N-ESDRERR]; NASA GES DISC
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.
The TMPA 3B42 data were provided by the NASA/Goddard Space Flight
Center's Mesoscale Atmospheric Processes Laboratory and Precipitation
Processing System (PPS), which develop and compute the TMPA as a
contribution to TRMM. Thanks extend to the anonymous reviewers for their
constructive comments.
NR 28
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Z9 10
U1 1
U2 17
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD SEP 15
PY 2015
VL 163
SI SI
BP 91
EP 101
DI 10.1016/j.atmosres.2014.12.015
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CK4HE
UT WOS:000356184100009
ER
PT J
AU Benafan, O
Garg, A
Noebe, RD
Bigelow, GS
Padula, SA
Gaydosh, DJ
Vaidyanathan, R
Clausen, B
Vogel, SC
AF Benafan, O.
Garg, A.
Noebe, R. D.
Bigelow, G. S.
Padula, S. A., II
Gaydosh, D. J.
Vaidyanathan, R.
Clausen, B.
Vogel, S. C.
TI Thermomechanical behavior and microstructural evolution of a Ni(Pd)-rich
Ni24.3Ti49.7Pd26 high temperature shape memory alloy
SO JOURNAL OF ALLOYS AND COMPOUNDS
LA English
DT Article
DE High temperature shape memory alloy; Neutron diffraction; NiTiPd;
Actuation; Two-way shape memory effect
ID TRANSMISSION ELECTRON-MICROSCOPY; SEVERE PLASTIC-DEFORMATION; TI-PD;
MARTENSITIC-TRANSFORMATION; MECHANICAL-PROPERTIES; PHASE-TRANSFORMATION;
CYCLIC ACTUATION; TEXTURE ANALYSIS; SITE PREFERENCE; NITI
AB The effect of thermomechanical cycling on a slightly Ni(Pd)-rich Ni24.3Ti49.7Pd26 (near stochiometric Ni-Ti basis with Pd replacing Ni) high temperature shape memory alloy was investigated. Aged tensile specimens (400 degrees C/24 h/furnace cooled) were subjected to constant-stress thermal cycling in conjunction with microstructural assessment via in situ neutron diffraction and transmission electron microscopy (TEM), before and after testing. It was shown that in spite of the slightly Ni(Pd)-rich composition and heat treatment used to precipitation harden the alloy, the material exhibited dimensional instabilities with residual strain accumulation reaching 1.5% over 10 thermomechanical cycles. This was attributed to insufficient strengthening of the material (insufficient volume fraction of precipitate phase) to prevent plasticity from occurring concomitant with the martensitic transformation. In situ neutron diffraction revealed the presence of retained martensite while cycling under 300 MPa stress, which was also confirmed by transmission electron microscopy of post-cycled samples. Neutron diffraction analysis of the post-thermally-cycled samples under no-load revealed residual lattice strains in the martensite and austenite phases, remnant texture in the martensite phase, and peak broadening of the austenite phase. Texture developed in the martensite phase was composed mainly of those martensitic tensile variants observed during thermomechanical cycling. Presence of a high density of dislocations, deformation twins, and retained martensite was revealed in the austenite state via in-situ TEM in the post-cycled material, providing an explanation for the observed peak broadening in the neutron diffraction spectra. Despite the dimensional instabilities, this alloy exhibited a biased transformation strain on the order of 3% and a two-way shape memory effect (TWSME) strain of similar to 2%, at relatively high actuation temperatures. Published by Elsevier B.V.
C1 [Benafan, O.; Garg, A.; Noebe, R. D.; Bigelow, G. S.; Padula, S. A., II; Gaydosh, D. J.] NASA Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Garg, A.] Univ Toledo, Toledo, OH 43606 USA.
[Gaydosh, D. J.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Vaidyanathan, R.] Univ Cent Florida, Mat Sci & Engn Dept, Adv Mat Proc & Anal Ctr, Orlando, FL 32816 USA.
[Clausen, B.; Vogel, S. C.] Los Alamos Natl Lab, Div Mat Sci & Technol, 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
RI Clausen, Bjorn/B-3618-2015
OI Clausen, Bjorn/0000-0003-3906-846X
FU NASA Fundamental Aeronautics Program; Aeronautical Sciences and
Transformative Aeronautics Concepts Program; Transformational Tools and
Technologies Projects; Office of Basic Energy Sciences DOE; DOE
[DE-AC52-06NA25396]
FX Funding from the NASA Fundamental Aeronautics Program, Aeronautical
Sciences and Transformative Aeronautics Concepts Program,
Transformational Tools and Technologies Projects, technical lead Dale
Hopkins, is gratefully acknowledged. The authors thank T.A. Sisneros and
D. W. Brown at LANL for technical support and helpful discussions. The
authors also thank D.F. Johnson for conducting ICP measurements. This
work has benefited from the use of the SMARTS and HIPPO instruments at
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 under Contract No. DE-AC52-06NA25396.
NR 89
TC 1
Z9 1
U1 4
U2 43
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0925-8388
EI 1873-4669
J9 J ALLOY COMPD
JI J. Alloy. Compd.
PD SEP 15
PY 2015
VL 643
BP 275
EP 289
DI 10.1016/j.jallcom.2015.04.081
PG 15
WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy &
Metallurgical Engineering
SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering
GA CJ0EZ
UT WOS:000355149300039
ER
PT J
AU Theiling, BP
Coleman, M
AF Theiling, Bethany P.
Coleman, Max
TI Refining the extraction methodology of carbonate associated sulfate:
Evidence from synthetic and natural carbonate samples
SO CHEMICAL GEOLOGY
LA English
DT Article
DE Carbonate associated sulfate; CAS; Sulfur isotopes; Pyrite oxidation;
Extraction; Oxygen isotopes
ID SULFUR ISOTOPIC COMPOSITION; MIOCENE MONTEREY FORMATION; SEAWATER
SULFATE; OXYGEN ISOTOPES; OXIDATION; PYRITE; FRACTIONATION; DELTA-S-34;
REDUCTION; BOUNDARY
AB Sulfur and oxygen isotope analyses of trace and whole mineral sulfate are valuable in investigating diagenetic processes and the microbial communities that produced them, seawater anoxia, and paleoclimate. Oxygen isotopes are particularly useful in that they may also record alterations to the original isotope ratio, be it from post-depositional processes or oxidation of sulfide minerals during the chemical extraction procedure. Here we rigorously test several common methodological procedures of extracting carbonate associated sulfate (CAS) for sulfur and oxygen isotope analyses in order to generate a method that will extract only the CAS, while preserving associated organic reduced sulfur and sulfides for analysis. The results of these experiments on synthetically generated carbonates demonstrate that our proposed protocol sufficiently removes all non-CAS sulfate and does not result in oxidation of included sulfides. Analytical reproducibility (standard deviation) of synthetic carbonates is 0.1% (1 sigma) for delta S-34 and 0.3 parts per thousand (1 sigma) for delta O-18. Extractions of low pyrite, high organic matter geologic samples from the Monterey Formation across a range of facies types demonstrate a reproducibility (1 sigma) of 0.4 parts per thousand-0.7 parts per thousand for delta S-34 and 0.8 parts per thousand-1.3 parts per thousand for delta O-18, resulting from sample heterogeneity. delta S-34 and delta O-18 from Monterey Formation samples do not demonstrate oxidation of organic matter, suggesting our proposed protocol will preserve organic sulfur. A high pyrite-concentration Jet Rock concretion demonstrates that additional sulfate can be produced during the non-CAS leaching processes from oxidation of pyrite. We show that pyrite from the Jet Rock concretion ceases to oxidize when the sample is leached under an anoxic environment. (C) 2015 Elsevier B.V. All rights reserved.
C1 CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
NASA, Astrobiol Inst, Washington, DC USA.
RP Theiling, BP (reprint author), Univ Tulsa, Dept Geosci, 800 Tucker Dr, Tulsa, OK 74101 USA.
EM bethany-theiling@utulsa.edu
FU NASA Astrobiology Institute
FX We would like to thank Jim Boles for his assistance collecting samples
from the Monterey Formation and Sean Loyd for his guidance in accessing
the Naples Beach outcrops of the Monterey Formation. We are grateful for
the comments and suggestions from Simon Bottrell and an anonymous
reviewer, which considerably improved the focus of the manuscript. This
research was carried out at the Jet Propulsion Laboratory (JPL),
California Institute of Technology, under contract with the National
Aeronautics and Space Administration (NASA), and supported by the NASA
Astrobiology Institute (CAN 6, Wisconsin Astrobiology Research
Consortium).
NR 58
TC 2
Z9 2
U1 3
U2 13
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2541
EI 1878-5999
J9 CHEM GEOL
JI Chem. Geol.
PD SEP 14
PY 2015
VL 411
BP 36
EP 48
DI 10.1016/j.chemgeo.2015.06.018
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CP6SK
UT WOS:000360018300005
ER
PT J
AU Smith, R
Li, JM
Muller, A
Salama, F
AF Smith, Randall
Li, Jia-Ming
Mueller, Alfred
Salama, Farid
TI Special issue on atomic & molecular data for astrophysicists
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Editorial Material
C1 [Smith, Randall] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Li, Jia-Ming] Shandong Jiaotong Univ, Jinan, Peoples R China.
[Mueller, Alfred] Univ Giessen, Inst Atom & Mol Phys, Giessen, Germany.
[Salama, Farid] NASA Ames Res Ctr, Space Sci & Astrobiol Div, Mountain View, CA USA.
RP Smith, R (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RI Muller, Alfred/A-3548-2009;
OI Muller, Alfred/0000-0002-0030-6929; Smith, Randall/0000-0003-4284-4167;
Salama, Farid/0000-0002-6064-4401
NR 0
TC 0
Z9 0
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
EI 1361-6455
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD SEP 14
PY 2015
VL 48
IS 17
SI SI
AR 170201
DI 10.1088/0953-4075/48/17/170201
PG 1
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA CP1BE
UT WOS:000359610000001
ER
PT J
AU Liske, J
Baldry, IK
Driver, P
Tuffs, RJ
Alpaslan, M
Andrae, E
Brough, S
Cluver, ME
Grootes, MW
Gunawardhana, MLP
Kelvin, LS
Loveday, J
Robotham, ASG
Taylor, EN
Bamford, SP
Bland-Hawthorn, J
Brown, MJI
Drinkwater, MJ
Hopkins, AM
Meyer, MJ
Norberg, P
Peacock, JA
Agius, NK
Andrews, SK
Bauer, AE
Ching, JHY
Colless, M
Conselice, CJ
Croom, SM
Davies, LJM
De Propris, R
Dunne, L
Eardley, EM
Ellis, S
Foster, C
Frenk, CS
Haussler, B
Holwerda, BW
Howlett, C
Ibarra, H
Jarvis, MJ
Jones, DH
Kafle, PR
Lacey, CG
Lange, R
Lara-Lopez, MA
Lopez-Sanchez, AR
Maddox, S
Madore, BF
McNaught-Roberts, T
Moffett, AJ
Nichol, RC
Owers, MS
Palamara, D
Penny, SJ
Phillipps, S
Pimbblet, KA
Popescu, CC
Prescott, M
Proctor, R
Sadler, EM
Sansom, AE
Seibert, M
Sharp, R
Sutherland, W
Vazquez-Mata, JA
van Kampen, E
Wilkins, SM
Williams, R
Wright, AH
AF Liske, J.
Baldry, I. K.
Driver, P.
Tuffs, R. J.
Alpaslan, M.
Andrae, E.
Brough, S.
Cluver, M. E.
Grootes, M. W.
Gunawardhana, M. L. P.
Kelvin, L. S.
Loveday, J.
Robotham, A. S. G.
Taylor, E. N.
Bamford, S. P.
Bland-Hawthorn, J.
Brown, M. J. I.
Drinkwater, M. J.
Hopkins, A. M.
Meyer, M. J.
Norberg, P.
Peacock, J. A.
Agius, N. K.
Andrews, S. K.
Bauer, A. E.
Ching, J. H. Y.
Colless, M.
Conselice, C. J.
Croom, S. M.
Davies, L. J. M.
De Propris, R.
Dunne, L.
Eardley, E. M.
Ellis, S.
Foster, C.
Frenk, C. S.
Haessler, B.
Holwerda, B. W.
Howlett, C.
Ibarra, H.
Jarvis, M. J.
Jones, D. H.
Kafle, P. R.
Lacey, C. G.
Lange, R.
Lara-Lopez, M. A.
Lopez-Sanchez, A. R.
Maddox, S.
Madore, B. F.
McNaught-Roberts, T.
Moffett, A. J.
Nichol, R. C.
Owers, M. S.
Palamara, D.
Penny, S. J.
Phillipps, S.
Pimbblet, K. A.
Popescu, C. C.
Prescott, M.
Proctor, R.
Sadler, E. M.
Sansom, A. E.
Seibert, M.
Sharp, R.
Sutherland, W.
Vazquez-Mata, J. A.
van Kampen, E.
Wilkins, S. M.
Williams, R.
Wright, A. H.
TI Galaxy And Mass Assembly (GAMA): end of survey report and data release 2
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; galaxies: distances and redshifts; galaxies: fundamental
parameters; galaxies: general; galaxies: photometry; galaxies:
statistics
ID DIGITAL SKY SURVEY; STAR-FORMING GALAXIES; OSCILLATION SPECTROSCOPIC
SURVEY; SPECTRAL ENERGY-DISTRIBUTION; REDSHIFT SURVEY; LUMINOSITY
FUNCTION; STELLAR MASS; SDSS-III; ELLIPTIC GALAXIES; PHYSICAL-PROPERTIES
AB The Galaxy And Mass Assembly (GAMA) survey is one of the largest contemporary spectroscopic surveys of low redshift galaxies. Covering an area of similar to 286 deg(2) (split among five survey regions) down to a limiting magnitude of r < 19.8 mag, we have collected spectra and reliable redshifts for 238 000 objects using the AAOmega spectrograph on the Anglo-Australian Telescope. In addition, we have assembled imaging data from a number of independent surveys in order to generate photometry spanning the wavelength range 1 nm(-1) m. Here, we report on the recently completed spectroscopic survey and present a series of diagnostics to assess its final state and the quality of the redshift data. We also describe a number of survey aspects and procedures, or updates thereof, including changes to the input catalogue, redshifting and re-redshifting, and the derivation of ultraviolet, optical and near-infrared photometry. Finally, we present the second public release of GAMA data. In this release, we provide input catalogue and targeting information, spectra, redshifts, ultraviolet, optical and near-infrared photometry, single-component Sersic fits, stellar masses, H alpha-derived star formation rates, environment information, and group properties for all galaxies with r < 19.0 mag in two of our survey regions, and for all galaxies with r < 19.4 mag in a third region (72 225 objects in total). The data base serving these data is available at http://www.gama-survey.org/.
C1 [Liske, J.; van Kampen, E.] European So Observ, D-85748 Garching, Germany.
[Baldry, I. K.; Williams, R.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Driver, P.] Univ St Andrews, Sch Phys & Astron, Scottish Univ Phys Alliance, St Andrews KY16 9SS, Fife, Scotland.
[Driver, P.; Robotham, A. S. G.; Meyer, M. J.; Andrews, S. K.; Davies, L. J. M.; Lange, R.; Moffett, A. J.; Wright, A. H.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia.
[Tuffs, R. J.; Andrae, E.; Grootes, M. W.; Popescu, C. C.] Max Planck Inst Kernphys, Heidelberg, Germany.
[Alpaslan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Brough, S.; Bauer, A. E.; Ellis, S.; Foster, C.; Owers, M. S.] Australian Astron Observ, N Ryde, NSW 1670, Australia.
[Cluver, M. E.] Univ Western Cape, ZA-7535 Bellville, South Africa.
[Gunawardhana, M. L. P.; McNaught-Roberts, T.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Kelvin, L. S.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Loveday, J.; Howlett, C.; Vazquez-Mata, J. A.; Wilkins, S. M.] Univ Sussex, Dept Phys & Astron, Astron Ctr, Brighton BN1 9QH, E Sussex, England.
[Taylor, E. N.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia.
[Bamford, S. P.; Conselice, C. J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Bland-Hawthorn, J.; Ching, J. H. Y.; Croom, S. M.; Sadler, E. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Brown, M. J. I.; Palamara, D.; Penny, S. J.; Pimbblet, K. A.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Brown, M. J. I.; Palamara, D.; Penny, S. J.; Pimbblet, K. A.] Monash Univ, Monash Ctr Astrophys, Clayton, Vic 3800, Australia.
[Drinkwater, M. J.] Univ Queensland, Dept Phys, Brisbane, Qld 4072, Australia.
[Peacock, J. A.; Dunne, L.; Eardley, E. M.; Maddox, S.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Agius, N. K.; Popescu, C. C.; Sansom, A. E.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Colless, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[De Propris, R.] Univ Turku, Finnish Ctr Astron ESO, Pukkio 21500, Finland.
[Dunne, L.; Maddox, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand.
[Haessler, B.; Jarvis, M. J.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Haessler, B.] Univ Hertfordshire, Hatfield AL10 9AB, Herts, England.
[Holwerda, B. W.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Howlett, C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Ibarra, H.] Natl Inst Astrophys Opt & Elect, Puebla 72840, Mexico.
[Jarvis, M. J.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa.
[Jones, D. H.; Lopez-Sanchez, A. R.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia.
[Lara-Lopez, M. A.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Madore, B. F.; Seibert, M.] Carnegie Inst Sci, Observ, Pasadena, CA 91101 USA.
[Phillipps, S.] Univ Bristol, Sch Phys, Bristol BS8 1TL, Avon, England.
[Pimbblet, K. A.] Univ Hull, Dept Phys & Math, Kingston Upon Hull HU6 7RX, N Humberside, England.
[Popescu, C. C.] Romanian Acad, Astron Inst, Bucharest 040557, Romania.
[Proctor, R.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil.
[Sutherland, W.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England.
RP Liske, J (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM jliske@eso.org
RI Drinkwater, Michael/A-2201-2008; Bamford, Steven/E-8702-2010; Brown,
Michael/B-1181-2015;
OI Baldry, Ivan/0000-0003-0719-9385; Colless, Matthew/0000-0001-9552-8075;
Drinkwater, Michael/0000-0003-4867-0022; Bamford,
Steven/0000-0001-7821-7195; Brown, Michael/0000-0002-1207-9137; Kafle,
Prajwal Raj/0000-0002-3625-9546; Owers, Matt/0000-0002-2879-1663; Liske,
Jochen/0000-0001-7542-2927; Maddox, Stephen/0000-0001-5549-195X;
Robotham, Aaron/0000-0003-0429-3579; Alpaslan,
Mehmet/0000-0003-0321-1033; Sadler, Elaine/0000-0002-1136-2555; Foster,
Caroline/0000-0003-0247-1204
FU STFC (UK); ARC (Australia); AAO; Alfred P. Sloan Foundation; National
Science Foundation; US Department of Energy; National Aeronautics and
Space Administration; Japanese Monbukagakusho; Max Planck Society;
Higher Education Funding Council for England; American Museum of Natural
History; Astrophysical Institute Potsdam; University of Basel;
University of Cambridge; Case Western Reserve University; University of
Chicago; Drexel University; Fermilab; Institute for Advanced Study;
Japan Participation Group; Johns Hopkins University; Joint Institute for
Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and
Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST);
Los Alamos National Laboratory; Max-Planck-Institute for Astronomy
(MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State
University; Ohio State University; University of Pittsburgh; University
of Portsmouth; Princeton University; United States Naval Observatory;
University of Washington
FX GAMA is a joint European-Australasian project based around a
spectroscopic campaign using the AAT. The GAMA IC is based on data taken
from the SDSS and the UKIRT Infrared Deep Sky Survey. Complementary
imaging of the GAMA regions is being obtained by a number of independent
survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE,
Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is
funded by the STFC (UK), the ARC (Australia), the AAO, and the
participating institutions. The GAMA website is
http://www.gama-survey.org/.; Funding for the SDSS and SDSS-II has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Science Foundation, the US Department of
Energy, the National Aeronautics and Space Administration, the Japanese
Monbukagakusho, the Max Planck Society, and the Higher Education Funding
Council for England. The SDSS website is http://www.sdss.org/.; The SDSS
is managed by the Astrophysical Research Consortium for the
Participating Institutions. The Participating Institutions are the
American Museum of Natural History, Astrophysical Institute Potsdam,
University of Basel, University of Cambridge, Case Western Reserve
University, University of Chicago, Drexel University, Fermilab, the
Institute for Advanced Study, the Japan Participation Group, Johns
Hopkins University, the Joint Institute for Nuclear Astrophysics, the
Kavli Institute for Particle Astrophysics and Cosmology, the Korean
Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos
National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
Max-Planck-Institute for Astrophysics (MPA), New Mexico State
University, Ohio State University, University of Pittsburgh, University
of Portsmouth, Princeton University, the United States Naval
Observatory, and the University of Washington. Based on observations
made with the NASA Galaxy Evolution Explorer.; 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.
NR 134
TC 62
Z9 62
U1 2
U2 9
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 11
PY 2015
VL 452
IS 2
BP 2087
EP 2126
DI 10.1093/mnras/stv1436
PG 40
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8IW
UT WOS:000360851900078
ER
PT J
AU Dawson, T
Frey, S
Kelly, EF
Stafford, S
Schimel, D
AF Dawson, Todd
Frey, Serita
Kelly, Eugene F.
Stafford, Susan
Schimel, David
TI Illuminating next steps for NEON
SO SCIENCE
LA English
DT Letter
C1 [Dawson, Todd] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Frey, Serita] Univ New Hampshire, Dept Nat Resources, Durham, NH 03824 USA.
[Kelly, Eugene F.] Colorado State Univ, Dept Soil & Crop Sci, Ft Collins, CO 80523 USA.
[Stafford, Susan] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA.
[Schimel, David] Jet Prop Lab, Pasadena, CA 91101 USA.
RP Schimel, D (reprint author), Jet Prop Lab, Pasadena, CA 91101 USA.
EM dschimel@jpl.nasa.gov
NR 3
TC 0
Z9 0
U1 3
U2 9
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD SEP 11
PY 2015
VL 349
IS 6253
BP 1176
EP 1177
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CQ9XH
UT WOS:000360968400032
PM 26359396
ER
PT J
AU Arzoumanian, Z
Brazier, A
Burke-Spolaor, S
Chamberlin, SJ
Chatterjee, S
Christy, B
Cordes, JM
Cornish, NJ
Demorest, PB
Deng, X
Dolch, T
Ellis, JA
Ferdman, RD
Fonseca, E
Garver-Daniels, N
Jenet, F
Jones, G
Kaspi, VM
Koop, M
Lam, MT
Lazio, TJW
Levin, L
Lommen, AN
Lorimer, DR
Luo, J
Lynch, RS
Madison, DR
McLaughlin, MA
McWilliams, ST
Nice, DJ
Palliyaguru, N
Pennucci, TT
Ransom, SM
Siemens, X
Stairs, IH
Stinebring, DR
Stovall, K
Swiggum, J
Vallisneri, M
van Haasteren, R
Wang, Y
Zhu, WW
AF Arzoumanian, Z.
Brazier, A.
Burke-Spolaor, S.
Chamberlin, S. J.
Chatterjee, S.
Christy, B.
Cordes, J. M.
Cornish, N. J.
Demorest, P. B.
Deng, X.
Dolch, T.
Ellis, J. A.
Ferdman, R. D.
Fonseca, E.
Garver-Daniels, N.
Jenet, F.
Jones, G.
Kaspi, V. M.
Koop, M.
Lam, M. T.
Lazio, T. J. W.
Levin, L.
Lommen, A. N.
Lorimer, D. R.
Luo, J.
Lynch, R. S.
Madison, D. R.
McLaughlin, M. A.
McWilliams, S. T.
Nice, D. J.
Palliyaguru, N.
Pennucci, T. T.
Ransom, S. M.
Siemens, X.
Stairs, I. H.
Stinebring, D. R.
Stovall, K.
Swiggum, J.
Vallisneri, M.
van Haasteren, R.
Wang, Y.
Zhu, W. W.
CA NANOGrav Collaboration
TI NANOGrav CONSTRAINTS ON GRAVITATIONAL WAVE BURSTS WITH MEMORY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational waves; pulsars: general
ID PULSAR TIMING ARRAY; MILLISECOND PULSARS; 1ST DISCOVERIES; RADIATION;
PRECISION; LIMITS; SKY; J1713+0747; DISPERSION; ALPHA
AB Among efforts to detect gravitational radiation, pulsar timing arrays are uniquely poised to detect "memory" signatures, permanent perturbations in spacetime from highly energetic astrophysical events such as mergers of supermassive black hole binaries. The North American Nanohertz Observatory for Gravitational Waves (NANOGrav) observes dozens of the most stable millisecond pulsars using the Arecibo and Green Bank radio telescopes in an effort to study, among other things, gravitational wave memory. We herein present the results of a search for gravitational wave bursts with memory (BWMs) using the first five years of NANOGrav observations. We develop original methods for dramatically speeding up searches for BWM signals. In the directions of the sky where our sensitivity to BWMs is best, we would detect mergers of binaries with reduced masses of 109 M. out to distances of 30 Mpc; such massive mergers in the Virgo cluster would be marginally detectable. We find no evidence for BWMs. However, with our non-detection, we set upper limits on the rate at which BWMs of various amplitudes could have occurred during the time spanned by our data-e.g., BWMs with amplitudes greater than 10(-13) must encounter the Earth at a rate less than 1.5 yr(-1).
C1 [Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, XRay Astrophys Lab, Greenbelt, MD 20771 USA.
[Brazier, A.; Chatterjee, S.; Cordes, J. M.; Dolch, T.; Lam, M. T.; Madison, D. R.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Brazier, A.; Burke-Spolaor, S.; Demorest, P. B.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Chamberlin, S. J.; Siemens, X.] Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA.
[Brazier, A.; Christy, B.; Lommen, A. N.] Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA.
[Cornish, N. J.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
[Deng, X.; Koop, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Ellis, J. A.; Lazio, T. J. W.; Vallisneri, M.; van Haasteren, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
[Ferdman, R. D.; Kaspi, V. M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Fonseca, E.; Stairs, I. H.; Zhu, W. W.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Garver-Daniels, N.; Levin, L.; Lorimer, D. R.; McLaughlin, M. A.; McWilliams, S. T.; Palliyaguru, N.; Swiggum, J.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
[Jenet, F.; Luo, J.; Wang, Y.] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA.
[Jones, G.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Lynch, R. S.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Nice, D. J.] Lafayette Coll, Dept Phys, Easton, PA 18042 USA.
[Pennucci, T. T.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Stinebring, D. R.] Oberlin Coll, Dept Phys & Astron, Oberlin, OH 44074 USA.
[Stovall, K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
[Zhu, W. W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
RP Arzoumanian, Z (reprint author), NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
EM drm252@cornell.edu
OI Ransom, Scott/0000-0001-5799-9714; Nice, David/0000-0002-6709-2566
FU National Science Foundation (NSF) PIRE program [0968296]; NSERC;
Canadian Institute for Advanced Research; NANOGrav Physics Frontiers
Center NSF [PHYS-1430284]; New York Space Grant Consortium; NASA
[PF4-150120, PF3-140116]; JPL RTD program
FX We thank our anonymous referee for many thoughtful and thorough comments
that helped us to improve this manuscript. We thank T. Loredo for
helping us to appropriately treat extreme-value statistics and G. Hobbs
for his maintenance of and continual improvements to TEMPO2. The work of
Z.A., A.B., S.B.-S., S.J.C., S.C., B.C., N.J.C.J. M.C., P.B.D., T.D.,
J.A.E., N.G.-D., F.J., G.J., M.T.L., T.J.W.L., L.L., A.N.L., D.R.L.,
J.L., R.S.L., D.R.M., M.A.M., S.T.M., D.J.N., N.P.,T.T.P., S.M.R., X.S.,
D.R.S., K.S., J.S., M.V., R.vH. and Y.W. was partially supported through
the National Science Foundation (NSF) PIRE program award number 0968296.
NANOGrav research at UBC is supported by an NSERC Discovery Grant and
Discovery Accelerator Supplement and by the Canadian Institute for
Advanced Research. The work of the NANOGrav collaboration is partially
supported by the NANOGrav Physics Frontiers Center NSF Award
PHYS-1430284. D.R.M. acknowledges partial support through the New York
Space Grant Consortium. J.A.E. and R.vH. acknowledge support by NASA
through Einstein Fellowship grants PF4-150120 and PF3-140116,
respectively. M.V. acknowledges support from the JPL RTD program.
Portions of this research were carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. Parts of the analysis
in this work were carried out on the Nimrod cluster of S.M.R. Data for
this project were collected using the facilities of the National Radio
Astronomy Observatory and the Arecibo Observatory. The National Radio
Astronomy Observatory is a facility of the NSF operated under
cooperative agreement by Associated Universities, Inc. The Arecibo
Observatory is operated by SRI International under a cooperative
agreement with the NSF (AST-1100968), and in alliance with Ana G.
Mendez-Universidad Metropolitana and the Universities Space Research
Association.
NR 49
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2015
VL 810
IS 2
AR 150
DI 10.1088/0004-637X/810/2/150
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700066
ER
PT J
AU Atrio-Barandela, F
Kashlinsky, A
Ebeling, H
Fixsen, DJ
Kocevski, D
AF Atrio-Barandela, F.
Kashlinsky, A.
Ebeling, H.
Fixsen, D. J.
Kocevski, D.
TI PROBING THE DARK FLOW SIGNAL IN WMAP 9-YEAR AND PLANCK COSMIC MICROWAVE
BACKGROUND MAPS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; galaxies:
clusters: general; large-scale structure of the universe
ID SCALE PECULIAR VELOCITIES; BULK FLOW; GALAXIES; CLUSTERS; ANISOTROPY;
UNIVERSE; FLUCTUATIONS; RADIATION; DENSITY
AB The "dark flow" dipole is a statistically significant dipole found at the position of galaxy clusters in filtered maps of Cosmic Microwave Background (CMB) temperature anisotropies. The dipole measured in WMAP 3-, 5-, and 7-year data releases was (1) mutually consistent, (2) roughly aligned with the all-sky CMB dipole, and (3) correlated with clusters' X-ray luminosities. We analyzed WMAP 9 -year and. Planck 1st- year data releases using a catalog of 980 clusters outside of the Kp0 mask to test our earlier findings. The dipoles measured on these new data sets are fully compatible with our earlier estimates, are similar in amplitude and direction to our previous results, and are in disagreement with the results of an earlier study by the Planck Collaboration. Furthermore, in the Planck data sets dipoles are found to be independent of frequency, ruling out the thermal Sunyaev-Zeldovich as the source of the effect. In the data of both WMAP and Planck we find a clear correlation between the dipole measured at the cluster location in filtered maps and the average anisotropy on the original maps, further proving that the dipole is associated with clusters. The dipole signal is dominated by the most massive clusters, with a statistical significance that is better than 99%, slightly larger than in WMAP. Since both data sets differ in foreground contributions, instrumental noise, and other systematics, the agreement between the WMAP and Planck dipoles argues against them being due to systematic effects in either of the experiments.
C1 [Atrio-Barandela, F.] Univ Salamanca, Fis Teor, E-37008 Salamanca, Spain.
[Kashlinsky, A.; Fixsen, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kashlinsky, A.] Observat Cosmol Lab, SSAI, Greenbelt, MD 20771 USA.
[Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Fixsen, D. J.] Observat Cosmol Lab, UMCP, Greenbelt, MD 20771 USA.
[Kocevski, D.] Phys & Astron, Waterville, ME 04901 USA.
RP Atrio-Barandela, F (reprint author), Univ Salamanca, Fis Teor, E-37008 Salamanca, Spain.
EM atrio@usal.es; Alexander.Kashlinsky@nasa.gov; ebeling@ifa.hawaii.edu;
Dale.Fixsen@nasa.gov; dale.kocevski@colby.edu
RI Atrio-Barandela, Fernando/A-7379-2017
OI Atrio-Barandela, Fernando/0000-0002-2130-2513
FU Spanish Ministerio de Educacion y Ciencia [FIS2012-30926]
FX F.A.B. acknowledges financial support from the Spanish Ministerio de
Educacion y Ciencia (grant FIS2012-30926). We thank R. Genova-Santos for
providing the foreground-cleaned maps used in this work.
NR 37
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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 SEP 10
PY 2015
VL 810
IS 2
AR 143
DI 10.1088/0004-637X/810/2/143
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700059
ER
PT J
AU Bjoraker, GL
Wong, MH
de Pater, I
Adamkovics, M
AF Bjoraker, G. L.
Wong, M. H.
de Pater, I.
Adamkovics, M.
TI JUPITER'S DEEP CLOUD STRUCTURE REVEALED USING KECK OBSERVATIONS OF
SPECTRALLY RESOLVED LINE SHAPES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: gaseous
planets; planets and satellites: individual (Jupiter)
ID PROBE MASS-SPECTROMETER; WATER-VAPOR; AMMONIA ICE; DYNAMICAL
IMPLICATIONS; EQUATORIAL BELT; GIANT PLANETS; VOYAGER IRIS; ATMOSPHERE;
ABUNDANCE; COEFFICIENTS
AB Technique: We present a method to determine the pressure at which significant cloud opacity is present between 2 and 6 bars on Jupiter. We use (a) the strength of a Fraunhofer absorption line in a zone to determine the ratio of reflected sunlight to thermal emission, and (b) pressure-broadened line profiles of deuterated methane (CH3D) at 4.66 mu m to determine the location of clouds. We use radiative transfer models to constrain the altitude region of both the solar and thermal components of Jupiter's 5 mu m spectrum. Results: For nearly all latitudes on Jupiter the thermal component is large enough to constrain the deep cloud structure even when upper clouds are present. We find that hot spots, belts, and high latitudes have broader line profiles than do zones. Radiative transfer models show that hot spots in the North Equatorial Belt and South Equatorial Belt (SEB) typically do not have opaque clouds at pressures greater than 2 bars. The South Tropical Zone (STZ) at 32 degrees S has an opaque cloud top between 4 and 5 bars. From thermochemical models this must be a water cloud. We measured the variation of the equivalent width of CH3D with latitude for comparison with Jupiter's belt-zone structure. We also constrained the vertical profile of H2O in an SEB hot spot and in the STZ. The hot spot is very dry for P < 4.5 bars and then follows the H2O profile observed by the Galileo Probe. The STZ has a saturated H2O profile above its cloud top between 4 and 5 bars.
C1 [Bjoraker, G. L.] NASA, GSFC, Greenbelt, MD 20771 USA.
[Wong, M. H.; de Pater, I.; Adamkovics, M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Bjoraker, GL (reprint author), NASA, GSFC, Code 693, Greenbelt, MD 20771 USA.
EM gordon.l.bjoraker@nasa.gov
FU W. M. Keck Foundation; NASA Planetary Astronomy (PAST) Program
[NNX11AJ47G, NNX14AJ43G, NNX15AJ41G]; NASA Outer Planets Research
Program [NNX11AM55G]
FX The data presented were obtained at the W. M. Keck Observatory, which is
operated as a scientific partnership among the California Institute of
Technology, the University of California, and the National Aeronautics
and Space Administration. The Observatory was made possible by the
generous financial support of the W. M. Keck Foundation. The authors
extend special thanks to those of Hawaiian ancestry on whose sacred
mountain we are privileged to be guests. Without their generous
hospitality, none of the observations presented would have been
possible. We also would like to thank Linda Brown for steering us to the
latest broadening coefficients for CH3D. This research was supported by
the NASA Planetary Astronomy (PAST) Program grant number NNX11AJ47G,
NNX14AJ43G, NNX15AJ41G, and NASA Outer Planets Research Program grant
number NNX11AM55G.
NR 53
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U1 3
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2015
VL 810
IS 2
AR 122
DI 10.1088/0004-637X/810/2/122
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700038
ER
PT J
AU Boyer, ML
McDonald, I
Srinivasan, S
Zijlstra, A
van Loon, JT
Olsen, KAG
Sonneborn, G
AF Boyer, Martha L.
McDonald, Iain
Srinivasan, Sundar
Zijlstra, Albert
van Loon, Jacco Th.
Olsen, Knut A. G.
Sonneborn, George
TI IDENTIFICATION OF A CLASS OF LOW-MASS ASYMPTOTIC GIANT BRANCH STARS
STRUGGLING TO BECOME CARBON STARS IN THE MAGELLANIC CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: stars; Magellanic Clouds; stars: AGB and post-AGB; stars:
low-mass; stars: variables: general; stars: winds, outflows
ID LONG-PERIOD VARIABLES; GRAVITATIONAL LENSING EXPERIMENT.; POINT-SOURCE
CLASSIFICATION; SPITZER LEGACY PROGRAM; HIGH-REDSHIFT GALAXIES; OGLE-III
CATALOG; RICH AGB STARS; ALL-SKY SURVEY; EVOLVED STARS; DUST PRODUCTION
AB We have identified a new class of Asymptotic Giant Branch (AGB) stars in the Small and Large Magellanic Clouds (SMC/LMC) using optical to infrared photometry, light curves, and optical spectroscopy. The strong dust production and long-period pulsations of these stars indicate that they are at the very end of their AGB evolution. Period-mass-radius relations for the fundamental-mode pulsators give median current stellar masses of 1.14 M-circle dot in the LMC and 0.94 M-circle dot in the SMC (with dispersions of 0.21 and 0.18 M-circle dot, respectively), and models suggest initial masses of < 1.5 M-circle dot and < 1.25 M-circle dot, respectively. This new class of stars includes both O-rich and C-rich chemistries, placing the limit where dredge-up allows carbon star production below these masses. A high fraction of the brightest among them should show S star characteristics indicative of atmospheric C/O approximate to 1, and many will form O-rich dust prior to their C-rich phase. These stars can be separated from their less-evolved counterparts by their characteristically red J - [8] colors.
C1 [Boyer, Martha L.; Sonneborn, George] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Boyer, Martha L.] ORAU, Oak Ridge, TN 37831 USA.
[McDonald, Iain; Zijlstra, Albert] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Srinivasan, Sundar] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[van Loon, Jacco Th.] Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
[Olsen, Knut A. G.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RP Boyer, ML (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
EM martha.boyer@nasa.gov
FU NASA; NSF; University of California; JPL/California Institute of
Technology
FX We thank Paolo Ventura & Flavia Dell'Agli for providing their stellar
evolution tracks, and Amanda Karakas for providing dredge-up models. We
also thank Patricia Whitelock for helpful discussions on stellar
variability. This research made use of NASA's Astrophysics Data System;
the NASA/IPAC Infrared Science Archive, which is operated by
JPL/California Institute of Technology, under contract with the NASA;
the SIMBAD database, operated at CDS, Strasbourg, France; Astropy, a
community-developed core Python package for Astronomy (Astropy
Collaboration et al. 2013). This publication also makes use of data
products from the Two Micron All-Sky Survey, which is a joint project of
the University of Massachusetts and IPAC/California Institute of
Technology, funded by NASA and the NSF; and the Wide-field Infrared
Survey Explorer, which is a joint project of the University of
California, and the JPL/California Institute of Technology, funded by
NASA. M.L.B. is supported by the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by ORAU through a contract
with NASA.
NR 86
TC 8
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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 SEP 10
PY 2015
VL 810
IS 2
AR 116
DI 10.1088/0004-637X/810/2/116
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700032
ER
PT J
AU Camilo, F
Kerr, M
Ray, PS
Ransom, SM
Sarkissian, J
Cromartie, HT
Johnston, S
Reynolds, JE
Wolff, MT
Freire, PCC
Bhattacharyya, B
Ferrara, EC
Keith, M
Michelson, PF
Parkinson, PMS
Wood, KS
AF Camilo, F.
Kerr, M.
Ray, P. S.
Ransom, S. M.
Sarkissian, J.
Cromartie, H. T.
Johnston, S.
Reynolds, J. E.
Wolff, M. T.
Freire, P. C. C.
Bhattacharyya, B.
Ferrara, E. C.
Keith, M.
Michelson, P. F.
Parkinson, P. M. Saz
Wood, K. S.
TI PARKES RADIO SEARCHES OF FERMI GAMMA-RAY SOURCES AND MILLISECOND PULSAR
DISCOVERIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-rays: stars; pulsars: individual (PSR J0955-6150, PSR J1012-4235,
PSR J1036-8317, PSR J1903-7051, PSR J1946-5403)
ID LARGE-AREA TELESCOPE; X-RAY; SOURCE CATALOG; SPACE VELOCITIES; PSR
J1227-4853; BINARY PULSARS; NEUTRON-STAR; LAT; POLARIZATION; PULSATIONS
AB In a search with the Parkes radio telescope of 56 unidentified Fermi-Large Area Telescope (LAT) gamma-ray sources, we have detected 11 millisecond pulsars (MSPs), 10 of them discoveries, of which five were reported by Kerr et al. We did not detect radio pulsations from six other pulsars now known in these sources. We describe the completed survey, which included multiple observations of many targets conducted to minimize the impact of interstellar scintillation, acceleration effects in binary systems, and eclipses. We consider that 23 of the 39 remaining sources may still be viable pulsar candidates. We present timing solutions and polarimetry for five of the MSPs and gamma-ray pulsations for PSR J1903-7051 (pulsations for five others were reported in the second Fermi-LAT catalog of gamma-ray pulsars). Two of the new MSPs are isolated and five are in > 1 day circular orbits with 0.2-0.3 M. presumed white dwarf companions. PSR J0955-6150, in a 24 day orbit with a approximate to 0.25 M-circle dot companion but eccentricity of 0.11, belongs to a recently identified class of eccentric MSPs. PSR J1036-8317 is in an 8 hr binary with a > 0.14 M-circle dot companion that is probably a white dwarf. PSR J1946-5403 is in a 3 hr orbit with a > 0.02 M-circle dot companion with no evidence of radio eclipses.
C1 [Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Kerr, M.; Johnston, S.; Reynolds, J. E.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Kerr, M.; Wolff, M. T.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Sarkissian, J.] CSIRO Parkes Observ, Parkes, NSW 2870, Australia.
[Cromartie, H. T.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Freire, P. C. C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Bhattacharyya, B.; Keith, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Ferrara, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Michelson, P. F.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Michelson, P. F.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
RP Camilo, F (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
OI Ray, Paul/0000-0002-5297-5278; Ransom, Scott/0000-0001-5799-9714; Kerr,
Matthew/0000-0002-0893-4073
FU Commonwealth of Australia; National Aeronautics and Space Administration
(NASA); Department of Energy in the United States; Commissariat a
l'Energie Atomique; Centre National de la Recherche
Scientifique/Institut National de Physique Nucleaire et de Physique des
Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di
Fisica Nucleare in Italy; Ministry of Education, Culture, Sports,
Science and Technology (MEXT); High Energy Accelerator Research
Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan;
K. A. Wallenberg Foundation; Swedish Research Council; Swedish National
Space Board in Sweden
FX We are grateful to the wonderful staff at the Parkes telescope for their
role in making it such a flue research instrument. We thank in
particular the friends of the analog filterbank system, used to discover
more than 1000 pulsars, who staved off its demise long enough to allow
the completion of this work. We thank Willem van Straten and Paul
Demorest for their help with PSRCHIVE. The Parkes Observatory is part of
the Australia Telescope, which is funded by the Commonwealth of
Australia for operation as a National Facility managed by CSIRO.; The
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 a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council and the Swedish National Space Board in Sweden.
NR 67
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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 SEP 10
PY 2015
VL 810
IS 2
AR 85
DI 10.1088/0004-637X/810/2/85
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700001
ER
PT J
AU Christiansen, JL
Clarke, BD
Burke, CJ
Seader, S
Jenkins, JM
Twicken, JD
Catanzarite, JD
Smith, JC
Batalha, NM
Haas, MR
Thompson, SE
Campbell, JR
Sabale, A
Uddin, AKMK
AF Christiansen, Jessie L.
Clarke, Bruce D.
Burke, Christopher J.
Seader, Shawn
Jenkins, Jon M.
Twicken, Joseph D.
Catanzarite, Joseph D.
Smith, Jeffrey C.
Batalha, Natalie M.
Haas, Michael R.
Thompson, Susan E.
Campbell, Jennifer R.
Sabale, Anima
Uddin, A. K. M. Kamal
TI MEASURING TRANSIT SIGNAL RECOVERY IN THE KEPLER PIPELINE. II. DETECTION
EFFICIENCY AS CALCULATED IN ONE YEAR OF DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; techniques: photometric
ID SYSTEMATIC-ERROR CORRECTION; SUN-LIKE STARS; MISSION DATA;
PLANET-DETECTION; CANDIDATES; QUARTERS; SCIENCE; SAMPLE
AB The Kepler planet sample can only be used to reconstruct the underlying planet occurrence rate if the detection efficiency of the Kepler pipeline is known; here we present the results of a second experiment aimed at characterizing this detection efficiency. We inject simulated transiting planet signals into the pixel data of similar to 10,000 targets, spanning one year of observations, and process the pixels as normal. We compare the set of detections made by the pipeline with the expectation from the set of simulated planets, and construct a sensitivity curve of signal recovery as a function of the signal-to-noise of the simulated transit signal train. The sensitivity curve does not meet the hypothetical maximum detection efficiency; however, it is not as pessimistic as some of the published estimates of the detection efficiency. For the FGK stars in our sample, the sensitivity curve is well fit by a gamma function with the coefficients a = 4.35 and b = 1.05. We also find that the pipeline algorithms recover the depths and periods of the injected signals with very high fidelity, especially for periods longer than 10 days. We perform a simplified occurrence rate calculation using the measured detection efficiency compared to previous assumptions of the detection efficiency found in the literature to demonstrate the systematic error introduced into the resulting occurrence rates. The discrepancies in the calculated occurrence rates may go some way toward reconciling some of the inconsistencies found in the literature.
C1 [Christiansen, Jessie L.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91106 USA.
[Clarke, Bruce D.; Burke, Christopher J.; Seader, Shawn; Twicken, Joseph D.; Catanzarite, Joseph D.; Smith, Jeffrey C.; Thompson, Susan E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Jenkins, Jon M.; Batalha, Natalie M.; Haas, Michael R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Campbell, Jennifer R.; Sabale, Anima; Uddin, A. K. M. Kamal] NASA, Ames Res Ctr, Wyle Labs, Moffett Field, CA 94035 USA.
RP Christiansen, JL (reprint author), CALTECH, NASA, Exoplanet Sci Inst, M-S 100-22,770 S Wilson Ave, Pasadena, CA 91106 USA.
EM jessie.christiansen@caltech.edu
FU NASA's Science Mission Directorate; NASA [GRNASM99G000001]
FX Funding for the Kepler Discovery Mission is provided by NASA's Science
Mission Directorate. The authors acknowledge the efforts of the Kepler
Mission team for obtaining the calibrated pixels, light curves and data
validation diagnostics data used in this publication. These data
products were generated by the Kepler Mission science pipeline through
the efforts of the Kepler Science Operations Center and Science Office.
The Kepler Mission is lead by the project office at NASA Ames Research
Center. Ball Aerospace built the Kepler photometer and spacecraft which
is operated by the mission operations center at LASP. These data
products are archived at the Mikulski Archive for Space Telescopes and
the NASA Exoplanet Archive. J.L.C. is supported by NASA under award No.
GRNASM99G000001.
NR 33
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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 SEP 10
PY 2015
VL 810
IS 2
AR 95
DI 10.1088/0004-637X/810/2/95
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700011
ER
PT J
AU Karna, N
Zhang, J
Pesnell, WD
Webber, SAH
AF Karna, N.
Zhang, J.
Pesnell, W. Dean
Webber, S. A. Hess
TI STUDY OF THE 3D GEOMETRIC STRUCTURE AND TEMPERATURE OF A CORONAL CAVITY
USING THE LIMB SYNOPTIC MAP METHOD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: filaments, prominences; Sun: magnetic fields
ID WHOLE SUN MONTH; QUIESCENT FILAMENT; PROMINENCE CAVITY; MASS EJECTIONS;
DENSITIES; STREAMER; DYNAMICS; HINODE; HOLE
AB We present the three-dimensional geometric structure and thermal properties of a coronal cavity deduced from limb synoptic maps. The observations are extreme ultraviolet images from the Atmospheric Imager Assembly (AIA) and magnetic images from the Helioseismic Magnetic Imager instruments on board the Solar Dynamics Observatory. We describe a limb synoptic-map method used to effectively identify and measure cavities from annuli of radiance above the solar limb. We find that cavities are best seen in the 211, 193, and 171 angstrom passbands. The prominence associated with each cavity is best seen in the 304 angstrom synoptic maps. We also estimate the thermal properties of the cavity and surrounding plasma by combining the AIA radiances with a differential emission measure analysis. This paper focuses on one long cavity from a catalog of coronal cavities that we are developing. Cavities in this catalog are designated by a coded name using the Carrington Rotation number and position. Cavity C211347177N was observed during Carrington Rotation 2113 at the northwestern limb of the solar disk with an average latitude of 47 degrees N and a central longitude of 177 degrees. We showed the following. (1) The cavity is a long tube with an elliptical crosssection with ratios of the length to width and the length to height of 11: 1 and 7: 1, respectively. (2) The cavity is about 1360Mm long, or 170 degrees in longitude. (3) It is tilted in latitude. (4) And it is slightly hotter than its surroundings.
C1 [Karna, N.; Pesnell, W. Dean; Webber, S. A. Hess] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Karna, N.; Zhang, J.; Webber, S. A. Hess] George Mason Univ, Fairfax, VA 22030 USA.
RP Karna, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Pesnell, William/D-1062-2012;
OI Pesnell, William/0000-0002-8306-2500; Zhang, Jie/0000-0003-0951-2486
FU Schlumberger Foundation Faculty for the Future; Catholic University of
America; NASA's Solar Dynamics Observatory; NSF [AGS-1156120,
AGS-1249270]
FX N.K. thanks the Schlumberger Foundation Faculty for the Future for
supporting this research. S.A.H.W. thanks the Catholic University of
America and NASA's Solar Dynamics Observatory for supporting this
research. J.Z. is supported by NSF AGS-1156120 and NSF AGS-1249270. The
AIA and HMI data are courtesy of NASA/SDO and the AIA and HMI Science
Investigation Teams. The GMU AIA Synoptic Maps Dataset can be accessed
at http://spaceweather.gmu.edu/projects/synop/AIASM.html. We downloaded
and used paraview 4.1.0 from http://www.paraview.org/download/. The
referenced SolarSoft (SSW) software can be found at
www.lmsal.com/solarsoft. We would like to thank the anonymous referee,
whose insightful comments helped improve the paper.
NR 26
TC 2
Z9 2
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2015
VL 810
IS 2
AR 124
DI 10.1088/0004-637X/810/2/124
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700040
ER
PT J
AU Karna, N
Pesnell, WD
Zhang, J
AF Karna, N.
Pesnell, W. D.
Zhang, J.
TI APPEARANCES AND STATISTICS OF CORONAL CAVITIES DURING THE ASCENDING
PHASE OF SOLAR CYCLE 24
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: filaments, prominences; Sun: magnetic fields
ID POLAR MAGNETIC-FIELD; MERIDIONAL FLOW; FLUX TRANSPORT; MASS EJECTIONS;
REVERSAL; DYNAMICS; HOLE; SUN
AB We present a survey of 429 coronal prominence cavities found between 2010 May and 2015 February using the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly limb synoptic maps. We examined correlations between each cavity's height, width, and length. Our findings showed that around 38% of the cavities were prolate, 27% oblate, and 35% circular in shape. The lengths of the cavities ranged from 0.06 to 2.9 R-circle dot. When a cavity is longer than 1.5 R-circle dot, it has a narrower height range (0.1-0.3 R-circle dot), whereas when the cavity was shorter than 1.5 R-circle dot, it had a wider height range (0.07-0.5 R-circle dot). We find that the overall three-dimensional topology of the long, stable cavities can be characterized as a long tube with an elliptical cross section. We also noted that the circular and oblate cavities are longer in length than the prolate cavities. We also studied the physical mechanisms behind the cavity drift toward the pole and found it to be tied to the meridional flow. Finally, by observing the evolution of the cavity regions using SDO/Helioseismic Magnetic Imager (HMI) surface magnetic field observations, we found that the cavities formed a belt near the polar coronal hole boundary; we call this the cavity belt. Our results showed that the cavity belt migrated toward higher latitude over time and the cavity belt disappeared after the polar magnetic field reversal. This result shows that cavity evolution provides new insight into the solar cycle.
C1 [Karna, N.; Pesnell, W. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Karna, N.; Zhang, J.] George Mason Univ, Fairfax, VA 22030 USA.
RP Karna, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Pesnell, William/D-1062-2012;
OI Pesnell, William/0000-0002-8306-2500; Zhang, Jie/0000-0003-0951-2486
FU Schlumberger Foundation Faculty for the Future; NASA's Solar Dynamics
Observatory; NSF [AGS-1156120, AGS-1249270]
FX N.K. thanks the Schlumberger Foundation Faculty for the Future for
supporting this research. W.D.P. was supported by NASA's Solar Dynamics
Observatory. J.Z. is supported by NSF AGS-1156120 and NSF AGS-1249270.
The authors thank Sarah Gibson for many useful suggestions. The AIA and
HMI data are courtesy of NASA/SDO and the AIA and HMI Science
Investigation Teams. The GMU AIA Synoptic Maps Dataset can be accessed
at http://spaceweather.gmu.edu/projects/synop. The monthly international
sunspot numbers, separated by hemisphere, were obtained from
http://www.ngdc.noaa.gov/stp/space-weather/solar-data/solar-indices/suns
pot-numbers/hemispheric/lists/. Solar Polar Field Strength data,
separated by hemisphere were obtained from http://wso.stanford.edu. The
HMI synoptic maps were obtained from
http://jsoc.stanford.edu/data/hmi/synoptic/. We would like to thank the
anonymous referee for useful suggestions that helped improve the paper.
NR 29
TC 2
Z9 2
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2015
VL 810
IS 2
AR 123
DI 10.1088/0004-637X/810/2/123
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700039
ER
PT J
AU Laporte, N
Perez-Fournon, I
Calanog, JA
Cooray, A
Wardlow, JL
Bock, J
Bridge, C
Burgarella, D
Bussmann, RS
Cabrera-Lavers, A
Casey, CM
Clements, DL
Conley, A
Dannerbauer, H
Farrah, D
Fu, H
Gavazzi, R
Gonzalez-Solares, EA
Ivison, RJ
Lo Faro, B
Ma, B
Magdis, G
Marques-Chaves, R
Martinez-Navajas, P
Oliver, SJ
Osage, WA
Riechers, D
Rigopoulou, D
Scott, D
Streblyanska, A
Vieira, JD
AF Laporte, N.
Perez-Fournon, I.
Calanog, J. A.
Cooray, A.
Wardlow, J. L.
Bock, J.
Bridge, C.
Burgarella, D.
Bussmann, R. S.
Cabrera-Lavers, A.
Casey, C. M.
Clements, D. L.
Conley, A.
Dannerbauer, H.
Farrah, D.
Fu, H.
Gavazzi, R.
Gonzalez-Solares, E. A.
Ivison, R. J.
Lo Faro, B.
Ma, B.
Magdis, G.
Marques-Chaves, R.
Martinez-Navajas, P.
Oliver, S. J.
Osage, W. A.
Riechers, D.
Rigopoulou, D.
Scott, D.
Streblyanska, A.
Vieira, J. D.
TI ENVIRONMENT OF THE SUBMILLIMETER-BRIGHT MASSIVE STARBURST HFLS3 AT z
similar to 6.34
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: formation; galaxies: high-redshift; galaxies: luminosity
function, mass function; galaxies: starburst
ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; SPECTRAL
ENERGY-DISTRIBUTIONS; UV LUMINOSITY FUNCTIONS; DWARF/L-DWARF BINARIES;
HIGH-REDSHIFT GALAXIES; HUBBLE DEEP FIELD; DARK-MATTER MODEL; ALL-SKY
SURVEY; PHOTOMETRIC REDSHIFTS
AB We describe the search for Lyman. break galaxies (LBGs) near the submillimeter-bright starburst galaxy HFLS3 at z = 6.34 and a study on the environment of this massive galaxy during the end of reionization. We performed two independent selections of LBGs on images obtained with the Gran Telescopio Canarias (GTC) and the Hubble Space Telescope (HST) by combining nondetections in bands blueward of the Lyman. break and color selection. A total of 10 objects fulfilling the LBG selection criteria at z > 5.5 were selected over the 4.54 and 55.5 arcmin(2) covered by our HST and GTC images, respectively. The photometric redshift, UV luminosity, and star formation rate of these sources were estimated with models of their spectral energy distribution. These z similar to 6 candidates have physical properties and number densities in agreement with previous results. The UV luminosity function at z similar to 6 and a Voronoi tessellation analysis of this field show. no strong evidence for an overdensity of relatively bright objects (m(F105W) < 25.9) associated with HFLS3. However, the overdensity parameter deduced from this field and the surface density of objects cannot exclude. definitively the LBG overdensity hypothesis. Moreover, we identified three faint objects at less than 3 '' from HFLS3 with color consistent with those expected for z similar to 6 galaxies. Deeper data are needed to confirm their redshifts and to study their association with HFLS3 and the galaxy merger that may be responsible for the massive starburst.
C1 [Laporte, N.; Perez-Fournon, I.; Cabrera-Lavers, A.; Marques-Chaves, R.; Martinez-Navajas, P.; Streblyanska, A.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Laporte, N.; Perez-Fournon, I.; Cabrera-Lavers, A.; Marques-Chaves, R.; Martinez-Navajas, P.; Streblyanska, A.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Laporte, N.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 306 22, Chile.
[Calanog, J. A.; Cooray, A.; Casey, C. M.; Ma, B.; Osage, W. A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Cooray, A.; Bock, J.; Bridge, C.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Wardlow, J. L.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Burgarella, D.; Lo Faro, B.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, F-13013 Marseille, France.
[Bussmann, R. S.; Riechers, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Cabrera-Lavers, A.] GTC Project, E-38205 Tenerife, Spain.
[Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Conley, A.] Univ Colorado, CASA UCB 389, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Dannerbauer, H.] Univ Vienna, Inst Astron, A-1160 Vienna, Austria.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Fu, H.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Gavazzi, R.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Gonzalez-Solares, E. A.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England.
[Ivison, R. J.] European So Observ, D-85748 Garching, Germany.
[Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Magdis, G.; Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Oliver, S. J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Rigopoulou, D.] Rutherford Appleton Lab, Sci & Technol Facil Council, RAL Space, Didcot OX11 0QX, Oxon, England.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
RP Laporte, N (reprint author), Inst Astrofis Canarias, E-38200 Tenerife, Spain.
RI Magdis, Georgios/C-7295-2014; Ivison, R./G-4450-2011; Wardlow,
Julie/C-9903-2015;
OI Magdis, Georgios/0000-0002-4872-2294; Ivison, R./0000-0001-5118-1313;
Wardlow, Julie/0000-0003-2376-8971; Scott, Douglas/0000-0002-6878-9840;
Casey, Caitlin/0000-0002-0930-6466
FU Spanish MINECO [AYA2010-21697-C05-04, FIS2012-39162-C06-02]; Chilean
Basal-CATA [PFB-06/2007]; CONICYT-Chile under the grant Gemini-CONICYT
[32120003]; NASA through Space Telescope Science Institute under NASA
[HST-GO-13045, NAS 5-26555]; NSF [AST-1313319]; Danish National Research
Foundation; Science and Technology Facilities Council [ST/I000976/1,
ST/K00106X/1]; European Research Council in the form of Advanced Grant,
COSMICISM [321302]; CSA (Canada); NAOC (China); CEA (France); CNES
(France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC
(UK); UKSA (UK); NASA (USA)
FX Financial support for this work was provided by the LSpanish MINECO
under projects AYA2010-21697-C05-04 and FIS2012-39162-C06-02, by the
Chilean Basal-CATA PFB-06/2007 and CONICYT-Chile under the grant
Gemini-CONICYT #32120003, and by NASA through grant HST-GO-13045 from
the Space Telescope Science Institute, which is operated by Associated
Universities for Research in Astronomy, Inc., under NASA contract NAS
5-26555. Additional support for A.C., W.O., J.C., J.L.W., and C.M.C. was
from NSF with AST-1313319. The Dark Cosmology Centre is funded by the
Danish National Research Foundation ( J.L.W.). S.O. acknowledges support
from the Science and Technology Facilities Council [grant number
ST/I000976/1]. D.R. acknowledges support from the Science and Technology
Facilities Council (ST/K00106X/1). R.J.I. acknowledges support from the
European Research Council in the form of Advanced Grant, COSMICISM,
321302. 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); 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). We thank Jose
Acosta-Pulido for advice on the LIRIS observations and help with the
LIRIS data reduction package. This work is based on observations made
with the Gran Telescopio Canarias (GTC), installed in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofisica
de Canarias, on the island of La Palma. The William Herschel Telescope
is operated on the island of La Palma by the Isaac Newton Group in the
Spanish Observatorio del Roque de los Muchachos of the Instituto de
Astrofsica de Canarias. The data presented in this paper will be
released through the Herschel Database in Marseille HeDaM
(hedam.oamp.fr/HerMES)
NR 96
TC 0
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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 SEP 10
PY 2015
VL 810
IS 2
AR 130
DI 10.1088/0004-637X/810/2/130
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700046
ER
PT J
AU Lopez, RA
Navarro, RE
Moya, PS
Vinas, AF
Araneda, JA
Munoz, V
Valdivia, JA
AF Lopez, Rodrigo A.
Navarro, Roberto E.
Moya, Pablo S.
Vinas, Adolfo F.
Araneda, Jaime A.
Munoz, Victor
Alejandro Valdivia, J.
TI SPONTANEOUS ELECTROMAGNETIC FLUCTUATIONS IN A RELATIVISTIC MAGNETIZED
ELECTRON-POSITRON PLASMA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: analytical; methods: numerical; plasmas; radiation mechanisms:
thermal; relativistic processes; waves
ID PAIR PLASMA; PARTICLE-ACCELERATION; PULSAR MAGNETOSPHERES;
KINETIC-THEORY; THERMAL NOISE; SOLAR-WIND; RECONNECTION; CYCLOTRON;
WAVES; SIMULATIONS
AB Spontaneous fluctuations are a robust phenomenon of plasmas near equilibrium, which does not depend on the existence of instabilities, and their characterization provides valuable information about the role of the relativistic temperatures T similar to mc(2) in relativistic regimes. In this paper, we study the broadband spontaneous electromagnetic fluctuations in a relativistic and magnetized pair plasma described by Maxwell-Juttner distribution functions, based on the fluctuation-dissipation theorem and particle-in-cell simulations. It is shown that the transverse electromagnetic fluctuations are constrained by a temperature-independent critical frequency omega(c) = root Omega(2)(c) + (ck)(2), which separates the collisionless damping regime (vertical bar omega vertical bar < omega(c)) from the case where the waves can propagate without damping (vertical bar omega vertical bar > omega(c)). Further, relativistic simulations show an excellent agreement between analytical and numerical results. We expect this formalism to contribute to obtaining useful physical information about the state of relativistic plasmas.
C1 [Lopez, Rodrigo A.; Navarro, Roberto E.; Araneda, Jaime A.] Univ Concepcion, Fac Ciencias Fis & Matemat, Dept Fis, Concepcion, Chile.
[Moya, Pablo S.; Vinas, Adolfo F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Moya, Pablo S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Moya, Pablo S.; Munoz, Victor; Alejandro Valdivia, J.] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile.
[Alejandro Valdivia, J.] Ctr Desarrollo Nanociencia & Nanotecnol, Cedenna, Chile.
RP Lopez, RA (reprint author), Univ Concepcion, Fac Ciencias Fis & Matemat, Dept Fis, Casilla 160-C, Concepcion, Chile.
EM rlopez186@gmail.com
RI Moya, Pablo/C-3163-2011; Lopez, Rodrigo/H-7576-2013; Navarro,
Roberto/F-7045-2014; Valdivia, Juan/A-3631-2008; Munoz,
Victor/A-2255-2008
OI Moya, Pablo/0000-0002-9161-0888; Navarro, Roberto/0000-0003-0782-1904;
Valdivia, Juan/0000-0003-3381-9904;
FU CONICyT through FONDECyT [3140142, 3150262]; FONDECyT [1150718,
1130273]; Universidad de Concepcion through VRID-Enlace grant
[215.011.059-1.0]; CONICyT-Becas Chile program; CEDENNA; NASA-Wind/SWE
FX We are grateful for the support of CONICyT through FONDECyT Postdoctoral
grant Nos. 3140142 (R.A.L.) and No. 3150262 (R.E.N) and FONDECyT grant
Nos. 1150718 and 1130273 (J.A.V.). J.A.A. thanks the Universidad de
Concepcion for support through VRID-Enlace grant No. 215.011.059-1.0.
P.S.M. thanks the CONICyT-Becas Chile program for providing financial
support for a postdoctoral fellow. We also thank CEDENNA for financial
support. A.F.V. would like to thank the NASA-Wind/SWE project for their
support.
NR 68
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Z9 7
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 SEP 10
PY 2015
VL 810
IS 2
AR 103
DI 10.1088/0004-637X/810/2/103
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700019
ER
PT J
AU Rahoui, F
Tomsick, JA
Coriat, M
Corbel, S
Furst, F
Gandhi, P
Kalemci, E
Migliari, S
Stern, D
Tzioumis, AK
AF Rahoui, Farid
Tomsick, John A.
Coriat, Mickael
Corbel, Stephane
Fuerst, Felix
Gandhi, Poshak
Kalemci, Emrah
Migliari, Simone
Stern, Daniel
Tzioumis, Anastasios K.
TI OPTICAL AND NEAR-INFRARED SPECTROSCOPY OF THE BLACK HOLE SWIFT
J1753.5-0127
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; binaries: close; infrared: stars; ISM: jets
and outflows; stars: individual (Swift J1753.5-0127); X-rays: binaries
ID X-RAY BINARIES; COMPTON HEATED WINDS; INNER COOL DISKS; LOW-HARD STATE;
COMPACT JET; GX 339-4; ACCRETION DISKS; MULTIWAVELENGTH OBSERVATIONS;
RADIO-EMISSION; LOW/HARD STATE
AB We report on a multiwavelength observational campaign of the black hole (BH) X-ray binary Swift J1753.5-0127 that consists of an ESO/X-shooter spectrum supported by contemporaneous Swift/X-ray Telescope+Ultra-Violet/Optical Telescope (UVOT) and Australia Telescope Compact Array data. Interstellar medium. absorption lines in the X-shooter spectrum allow. us to determine E(B - V)= 0.45 +/- 0.02 along the line of sight to the source. We also report detection of emission signatures of He II lambda 4686, H alpha, and, for the first time, H I lambda 10906 and Pa beta. The double-peaked morphology of these four lines is typical of the chromosphere of a rotating accretion disk. Nonetheless, the paucity of disk features points toward a low level of irradiation in the system. This is confirmed through spectral energy distribution modeling, and we find that the UVOT+X-shooter continuum mostly stems from the thermal emission of a viscous disk. We speculate that the absence of reprocessing is due to the compactness of an illumination-induced envelope that fails to reflect enough incoming hard X-ray photons back to the outer regions. The disk also marginally contributes to the Compton-dominated X-ray emission and is strongly truncated, with an inner radius about 1000 times larger than the BH's gravitational radius. A near-infrared excess is present, and we associate it with synchrotron radiation from a compact jet. However, the measured X-ray flux is significantly higher than what can be explained by the optically thin synchrotron jet component. We discuss these findings in the framework of the radio-quiet versus X-ray-bright hypothesis, favoring the presence of a residual disk, predicted by evaporation models, that contributes to the X-ray emission without enhancing the radio flux.
C1 [Rahoui, Farid] European So Observ, K Schwarzschild Str 2, D-85748 Garching, Germany.
[Rahoui, Farid] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Coriat, Mickael] Univ Toulouse, UPS, IRAP, F-31028 Toulouse 4, France.
[Coriat, Mickael] CNRS, UMR5277, F-31028 Toulouse, France.
[Corbel, Stephane] Univ Paris Diderot, Lab AIM, CEA, IRFU,CNRS,INSU,DSM,SAp, F-91191 Gif Sur Yvette, France.
[Corbel, Stephane] Univ Orlans, PSL Res Univ, Stn Radioastron Nanay, Observ Paris,CNRS,OSUC, F-18330 Nanay, France.
[Fuerst, Felix] CALTECH, Pasadena, CA 91125 USA.
[Gandhi, Poshak] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Kalemci, Emrah] Sabanci Univ, TR-34956 Istanbul, Turkey.
[Migliari, Simone] European Space Astron Ctr, E-28691 Madrid, Spain.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tzioumis, Anastasios K.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
RP Rahoui, F (reprint author), European So Observ, K Schwarzschild Str 2, D-85748 Garching, Germany.
EM frahoui@eso.org
OI Rahoui, Farid/0000-0001-7655-4120
FU NASA [NNX13AJ81G, NNX14AC56G]; UnivEarthS Labex program of Sorbonne
Paris Cite [ANR-10-LABX-0023, ANR-11-IDEX-0005-02]; CHAOS project -
French Research National Agency [ANR-12-BS05-0009]; TUBITAK BIDEB
program [2219]; Spanish Ministerio de Economia y Competitividad (MINECO)
[AYA2013-47447-C3-1-P]; Planetary Science Division of the National
Aeronautics and Space Administration; Commonwealth of Australia
FX We thank the referee for very insightful and constructive comments. F.R.
thanks the ESO staff who performed the service observations. J.A.T.
acknowledges partial support from NASA under Swift Guest Observer grants
NNX13AJ81G and NNX14AC56G. S.C. acknowledges the financial support from
the UnivEarthS Labex program of Sorbonne Paris Cite (ANR-10-LABX-0023
and ANR-11-IDEX-0005-02) and from the CHAOS project ANR-12-BS05-0009
supported by the French Research National Agency. E.K. acknowledges
support from the TUBITAK BIDEB 2219 program. This work was supported by
the Spanish Ministerio de Economia y Competitividad (MINECO) under grant
AYA2013-47447-C3-1-P (S. M.). This research has made use of data
obtained from the High Energy Astrophysics Science Archive Research
Center (HEA-SARC), provided by NASA's Goddard Space Flight Center. This
publication also makes use of data products from NEOWISE, which is a
project of the Jet Propulsion Laboratory/California Institute of
Technology, funded by the Planetary Science Division of the National
Aeronautics and Space Administration. The Australia Telescope Compact
Array is part of the Australia Telescope, 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
and. of the SIMBAD. and VizieR databases operated at CDS, Strasbourg,
France.
NR 82
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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 SEP 10
PY 2015
VL 810
IS 2
AR 161
DI 10.1088/0004-637X/810/2/161
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700077
ER
PT J
AU Riguccini, L
Temi, P
Amblard, A
Fanelli, M
Brighenti, F
AF Riguccini, L.
Temi, P.
Amblard, A.
Fanelli, M.
Brighenti, F.
TI MID-IR ENHANCED GALAXIES IN THE COMA & VIRGO CLUSTERS: LENTICULARS WITH
A HIGH STAR FORMATION RATE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: elliptical and lenticular, cD;
galaxies: star formation
ID INFRARED-SURVEY-EXPLORER; TULLY-FISHER RELATION; SPITZER OBSERVATIONS;
ELLIPTIC GALAXIES; SPIRAL GALAXIES; S0 GALAXIES; XMM-NEWTON; ATLAS(3D)
PROJECT; DISTANT CLUSTERS; SAURON PROJECT
AB We explore the properties of early-type galaxies (ETGs), including ellipticals (E) and lenticulars (S0), in rich environments, such as clusters of galaxies (Virgo and Coma). The L-24/L-K distribution of ETGs in both Virgo and Coma clusters shows that some S0s have a much larger L-24/L-K ratio (0.5 to similar to 2 dex) than the bulk of the ETG population. This could be interpreted as an enhanced star formation rate in these lenticulars. We compare the optical colors of galaxies in these two clusters and investigate the nature of these sources with a large L-24/L-K ratio by looking at their spatial distribution within the cluster, analyzing their optical spectra, and looking at their optical colors compared to late-types. We obtain 10 Coma and 3 Virgo early-type sources with larger L-24/L-K ratios than the bulk of their population. We call these sources mid-infrared enhanced galaxies (MIEGs). In Coma, they are mostly located in the southwest part of the cluster where a substructure is falling onto the main cluster. MIEGs present a lower g-r color than the rest of the ETG sample because of a blue continuum. We interpret the excess L-24/L-K ratio as evidence for enhanced star formation induced as a consequence of their infall into the main cluster.
C1 [Riguccini, L.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, RJ, Brazil.
[Riguccini, L.; Amblard, A.; Fanelli, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Riguccini, L.; Temi, P.; Amblard, A.; Fanelli, M.] BAER Inst, Sonoma, CA USA.
[Brighenti, F.] Univ Bologna, Dept Astron, I-40127 Bologna, Italy.
RP Riguccini, L (reprint author), Univ Fed Rio de Janeiro, Observ Valongo, 43 Saude, BR-20080090 Rio De Janeiro, RJ, Brazil.
EM riguccini@astro.ufrj.br
FU NASA; National Aeronautics and Space Administration; Alfred P. Sloan
Foundation; National Science Foundation; U.S. Department of Energy
Office of Science; University of Arizona; Brazilian Participation Group;
Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon
University; University of Florida; French Participation Group; German
Participation Group; Harvard University; Instituto de Astrofisica de
Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns
Hopkins University; Lawrence Berkeley National Laboratory; Max Planck
Institute for Astrophysics; Max Planck Institute for Extraterrestrial
Physics; New Mexico State University; New York University; Ohio State
University; Pennsylvania State University; University of Portsmouth;
Princeton University; Spanish Participation Group; University of Tokyo;
University of Utah; Vanderbilt University; University of Virginia;
University of Washington; Yale University
FX This work is based on archival data obtained 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. This publication makes use of data
products from 2MASS, which is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology, funded by the National Aeronautics and Space
Administration and the National Science Foundation. This publication
makes use of data from SDSS-III. 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, University of Cambridge, Carnegie Mellon University,
University of Florida, the French Participation Group, the German
Participation Group, Harvard University, the Instituto de Astrofisica de
Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns
Hopkins University, Lawrence Berkeley National Laboratory, Max Planck
Institute for Astrophysics, Max Planck Institute for Extraterrestrial
Physics, New Mexico State University, New York University, Ohio State
University, Pennsylvania State University, University of Portsmouth,
Princeton University, the Spanish Participation Group, University of
Tokyo, University of Utah, Vanderbilt University, University of
Virginia, University of Washington, and Yale University.
NR 86
TC 2
Z9 2
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2015
VL 810
IS 2
AR 138
DI 10.1088/0004-637X/810/2/138
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700054
ER
PT J
AU Timokhin, AN
Harding, AK
AF Timokhin, A. N.
Harding, A. K.
TI ON THE POLAR CAP CASCADE PAIR MULTIPLICITY OF YOUNG PULSARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; plasmas; pulsars: general; stars: neutron
ID GAMMA-RAY PULSARS; ROTATION-POWERED PULSARS; AREA TELESCOPE CATALOG;
STRONG MAGNETIC-FIELDS; NEUTRON-STAR SURFACE; CRAB-NEBULA; WIND NEBULAE;
LIGHT CURVES; LOW-ALTITUDE; CURRENT FLOW
AB We study the efficiency of pair production in polar caps of young pulsars under a variety of conditions to estimate the maximum possible multiplicity of pair plasma in pulsar magnetospheres. We develop a semi-analytic model for calculation of cascade multiplicity which allows efficient exploration of the parameter space and corroborate it with direct numerical simulations. Pair creation processes are considered separately from particle acceleration in order to assess different factors affecting cascade efficiency, with acceleration of primary particles described by recent self-consistent non-stationary model of pair cascades. We argue that the most efficient cascades operate in the curvature radiation/synchrotron regime, the maximum multiplicity of pair plasma in pulsar magnetospheres is similar to few x 10(5). The multiplicity of pair plasma in magnetospheres of young energetic pulsars weakly depends on the strength of the magnetic field and the radius of curvature of magnetic field lines and has a stronger dependence on pulsar inclination angle. This result questions assumptions about very high pair plasma multiplicity in theories of pulsar wind nebulae.
C1 [Timokhin, A. N.; Harding, A. K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Timokhin, A. N.] Univ Maryland, Coll Pk UMDCP CRESST, College Pk, MD 20742 USA.
RP Timokhin, AN (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
EM andrey.timokhin@nasa.gov
FU NASA Astrophysics Theory grant; Fermi Cycle-5 guest investigator grant
FX This work was supported by a NASA Astrophysics Theory grant and a Fermi
Cycle-5 guest investigator grant.
NR 51
TC 9
Z9 9
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 SEP 10
PY 2015
VL 810
IS 2
AR 144
DI 10.1088/0004-637X/810/2/144
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700060
ER
PT J
AU Yee, JC
Gould, A
Beichman, C
Novati, SC
Carey, S
Gaudi, BS
Henderson, CB
Nataf, D
Penny, M
Shvartzvald, Y
Zhu, W
AF Yee, Jennifer C.
Gould, Andrew
Beichman, Charles
Novati, Sebastiano Calchi
Carey, Sean
Gaudi, B. Scott
Henderson, Calen B.
Nataf, David
Penny, Matthew
Shvartzvald, Yossi
Zhu, Wei
TI CRITERIA FOR SAMPLE SELECTION TO MAXIMIZE PLANET SENSITIVITY AND YIELD
FROM SPACE-BASED MICROLENS PARALLAX SURVEYS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing: micro
ID SPITZER OBSERVATIONS; MACHO PARALLAXES; MASS MEASUREMENT; GALACTIC
BULGE; PROPER MOTIONS; SATELLITE MASS; GAS GIANTS; MILKY-WAY; EVENTS;
STAR
AB Space-based microlens parallax measurements are a powerful tool for understanding planet populations, especially their distribution throughout the Galaxy. However, if space-based observations of the microlensing events must be specifically targeted, it is crucial that microlensing events enter the parallax sample without reference to the known presence or absence of planets. Hence, it is vital to define objective criteria for selecting events where possible and to carefully consider and minimize the selection biases where not possible so that the final sample represents a controlled experiment. We present objective criteria for initiating observations and determining their cadence for a subset of events, and we define procedures for isolating subjective decision making from information about detected planets for the remainder of events. We also define procedures to resolve conflicts between subjective and objective selections. These procedures maximize the planet sensitivity of the sample as a whole by allowing for planet detections even if they occur before satellite observations for objectively selected events and by helping to trigger fruitful follow-up observations for subjectively chosen events. This paper represents our public commitment to these procedures, which is a necessary component of enforcing objectivity on the experimental protocol. They will be implemented for the 2015 Spitzer microlensing campaign.
C1 [Yee, Jennifer C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gould, Andrew; Gaudi, B. Scott; Henderson, Calen B.; Penny, Matthew] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Beichman, Charles; Novati, Sebastiano Calchi] NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Novati, Sebastiano Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy.
[Novati, Sebastiano Calchi] IIASS, I-84019 Vietri Sul Mare, SA, Italy.
[Carey, Sean] CALTECH, Ctr Sci, Spitzer, Pasadena, CA 91125 USA.
[Nataf, David] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Shvartzvald, Yossi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
RP Yee, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU JPL grant [1500811]; California Institute of Technology (Caltech)/Jet
Propulsion Laboratory (JPL) - NASA through the Sagan Fellowship Program;
Australian Research Council [FL110100012]
FX Work by J.C.Y., A.G., and S.C. was supported by JPL grant 1500811. Work
by J.C.Y. was performed under contract with the California Institute of
Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA
through the Sagan Fellowship Program executed by the NASA Exoplanet
Science Institute. D.M.N. was supported by the Australian Research
Council grant FL110100012.
NR 40
TC 12
Z9 12
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 SEP 10
PY 2015
VL 810
IS 2
AR 155
DI 10.1088/0004-637X/810/2/155
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS4ZA
UT WOS:000362083700071
ER
PT J
AU Huerta, EA
McWilliams, ST
Gair, JR
Taylor, SR
AF Huerta, E. A.
McWilliams, Sean T.
Gair, Jonathan R.
Taylor, Stephen R.
TI Detection of eccentric supermassive black hole binaries with pulsar
timing arrays: Signal-to-noise ratio calculations
SO PHYSICAL REVIEW D
LA English
DT Article
ID GRAVITATIONAL-WAVE SIGNAL; ACTIVE GALACTIC NUCLEI; GALAXY MERGERS;
LOW-FREQUENCY; STELLAR-SYSTEMS; ORBITAL DECAY; GAS; RADIATION;
EVOLUTION; LIMITS
AB We present a detailed analysis of the expected signal-to-noise ratios of supermassive black hole binaries on eccentric orbits observed by pulsar timing arrays. We derive several analytical relations that extend the results of Peters and Mathews [Phys. Rev. D 131, 435 (1963)] to quantify the impact of eccentricity in the detection of single resolvable binaries in the pulsar timing array band. We present ready-to-use expressions to compute the increase/loss in signal-to-noise ratio of eccentric single resolvable sources whose dominant harmonic is located in the low/high frequency sensitivity regime of pulsar timing arrays. Building upon the work of Phinney (arXiv:astro-ph/0108028) and Enoki and Nagashima [Prog. Theor. Phys. 117, 241 (2007)], we present an analytical framework that enables the construction of rapid spectra for a stochastic gravitational-wave background generated by a cosmological population of eccentric sources. We confirm previous findings which indicate that, relative to a population of quasicircular binaries, the strain of a stochastic, isotropic gravitational-wave background generated by a cosmological population of eccentric binaries will be suppressed in the frequency band of pulsar timing arrays. We quantify this effect in terms of signal-to-noise ratios in a pulsar timing array.
C1 [Huerta, E. A.; McWilliams, Sean T.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
[Gair, Jonathan R.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Taylor, Stephen R.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
[Huerta, E. A.] Univ Illinois, NCSA, Urbana, IL 61801 USA.
[Gair, Jonathan R.] Univ Edinburgh, Sch Math, Edinburgh EH9 3JZ, Midlothian, Scotland.
RP Huerta, EA (reprint author), W Virginia Univ, Dept Phys & Astron, White Hall, Morgantown, WV 26506 USA.
EM elihu@illinois.edu
OI Taylor, Stephen/0000-0003-0264-1453
FU Royal Society; NASA; National Science Foundation [PHYS-1066293];
hospitality of the Aspen Center for Physics
FX D J. G.'s work is supported by the Royal Society. This research was in
part supported by S. T.'s appointment to the NASA Postdoctoral Program
at the Jet Propulsion Laboratory, administered by Oak Ridge Associated
Universities through a contract with NASA. We thank Joe Romano for
kindly sharing with us his personal notes on the targeted sensitivity of
PTAs, which formed the basis of Ref. [89], and Chris Moore for verifying
that the dimensionless effective noise amplitude for continuous-wave
sources scales as similar to f-2 in the low frequency regime.
This work was supported in part by National Science Foundation Grant No.
PHYS-1066293 and the hospitality of the Aspen Center for Physics.
NR 96
TC 6
Z9 6
U1 0
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD SEP 10
PY 2015
VL 92
IS 6
AR 063010
DI 10.1103/PhysRevD.92.063010
PG 17
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CQ9VN
UT WOS:000360963400004
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
(vol 16, 053025, 2015)
SO NEW JOURNAL OF PHYSICS
LA English
DT Correction
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
NR 1
TC 1
Z9 1
U1 2
U2 3
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 SEP 9
PY 2015
VL 17
AR 099501
DI 10.1088/1367-2630/17/9/099501
PG 1
WC Physics, Multidisciplinary
SC Physics
GA CZ8NI
UT WOS:000367356000001
ER
PT J
AU Rodriguez, JAP
Kargel, JS
Baker, VR
Gulick, VC
Berman, DC
Fairen, AG
Linares, R
Zarroca, M
Yan, JG
Miyamoto, H
Glines, N
AF Rodriguez, J. Alexis P.
Kargel, Jeffrey S.
Baker, Victor R.
Gulick, Virginia C.
Berman, Daniel C.
Fairen, Alberto G.
Linares, Rogelio
Zarroca, Mario
Yan, Jianguo
Miyamoto, Hideaki
Glines, Natalie
TI Martian outflow channels: How did their source aquifers form, and why
did they drain so rapidly?
SO SCIENTIFIC REPORTS
LA English
DT Article
ID SUBSURFACE HYDROLOGY; NORTHERN LOWLANDS; ANCIENT OCEANS; MARS; WATER;
ICE; SURFACE; GROUNDWATER; CHRONOLOGY; BOUNDARY
AB Catastrophic floods generated similar to 3.2 Ga by rapid groundwater evacuation scoured the Solar System's most voluminous channels, the southern circum-Chryse outflow channels. Based on Viking Orbiter data analysis, it was hypothesized that these outflows emanated from a global Hesperian cryosphere-confined aquifer that was infused by south polar meltwater infiltration into the planet's upper crust. In this model, the outflow channels formed along zones of superlithostatic pressure generated by pronounced elevation differences around the Highland-Lowland Dichotomy Boundary. However, the restricted geographic location of the channels indicates that these conditions were not uniform Boundary. Furthermore, some outflow channel sources are too high to have been fed by south polar basal melting. Using more recent mission data, we argue that during the Late Noachian fluvial and glacial sediments were deposited into a clastic wedge within a paleo-basin located in the southern circum-Chryse region, which was then completely submerged under a primordial northern plains ocean. Subsequent Late Hesperian outflow channels were sourced from within these geologic materials and formed by gigantic groundwater outbursts driven by an elevated hydraulic head from the Valles Marineris region. Thus, our findings link the formation of the southern circum-Chryse outflow channels to ancient marine, glacial, and fluvial erosion and sedimentation.
C1 [Rodriguez, J. Alexis P.; Berman, Daniel C.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Rodriguez, J. Alexis P.; Gulick, Virginia C.; Glines, Natalie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kargel, Jeffrey S.; Baker, Victor R.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Gulick, Virginia C.; Glines, Natalie] SETI Inst, Mountain View, CA 94043 USA.
[Fairen, Alberto G.] Ctr Astrobiol, Madrid 28850, Spain.
[Fairen, Alberto G.] Cornell Univ, Dept Astron, Ithaca, NY 14850 USA.
[Linares, Rogelio; Zarroca, Mario] Autonomous Univ Barcelona, External Geodynam & Hydrogeol Grp, Dept Geol, E-08193 Barcelona, Spain.
[Yan, Jianguo] Wuhan Univ, State Key Lab Informat Engn Surveying Mapping & R, Wuhan 430070, Peoples R China.
[Miyamoto, Hideaki] Univ Tokyo, Univ Museum, Tokyo 1130033, Japan.
RP Rodriguez, JAP (reprint author), Planetary Sci Inst, 1700 East Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA.
EM alexis@psi.edu
RI Miyamoto, Hideaki/B-9666-2008;
OI Zarroca, Mario/0000-0001-6907-1892
FU NASA's NPP program; MRO HiRISE Co-Investigator funds; Project "icyMARS"
- European Research Council [307496]; KAKENHI [23340126]
FX We are grateful to James Head III for his insightful comments and
suggestions, which significantly improved the quality of this
manuscript. Funding provided by NASA's NPP program to J. Alexis P.
Rodriguez and by MRO HiRISE Co-Investigator funds to V.C. Gulick. A. G.
Fairen was supported by the Project "icyMARS", funded by the European
Research Council, Starting Grant no 307496. Hideaki Miyamoto was
supported by KAKENHI 23340126. We would also like to express our
gratitude to Alexander Cox for his helpful suggestions regarding the
editing of this paper. HiRISE images were analyzed using HiView
developed by the Lunar and Planetary Laboratory at the University of
Arizona.
NR 55
TC 6
Z9 6
U1 1
U2 14
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD SEP 8
PY 2015
VL 5
AR 13404
DI 10.1038/srep13404
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CQ7OA
UT WOS:000360792300001
PM 26346067
ER
PT J
AU Zhai, PW
Hu, YX
Winker, DM
Franz, BA
Boss, E
AF Zhai, Peng-Wang
Hu, Yongxiang
Winker, David M.
Franz, Bryan A.
Boss, Emmanuel
TI Contribution of Raman scattering to polarized radiation field in ocean
waters
SO OPTICS EXPRESS
LA English
DT Article
ID IN-SITU MEASUREMENTS; MUELLER MATRIX; UNDERWATER POLARIZATION;
OPTICAL-PROPERTIES; LEAVING RADIANCE; FRAUNHOFER LINES;
LIGHT-SCATTERING; NATURAL-WATERS; PHASE FUNCTION; MONTE-CARLO
AB We have implemented Raman scattering in a vector radiative transfer model for coupled atmosphere and ocean systems. A sensitivity study shows that the Raman scattering contribution is greatest in clear waters and at longer wavelengths. The Raman scattering contribution may surpass the elastic scattering contribution by several orders of magnitude at depth. The degree of linear polarization in water is smaller when Raman scattering is included. The orientation of the polarization ellipse shows similar patterns for both elastic and inelastic scattering contributions. As polarimeters and multipolarization-state lidars are planned for future Earth observing missions, our model can serve as a valuable tool for the simulation and interpretation of these planned observations. (C) 2015 Optical Society of America
C1 [Zhai, Peng-Wang] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Hu, Yongxiang; Winker, David M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Franz, Bryan A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Boss, Emmanuel] Univ Maine, Sch Marine Sci, Orono, ME 04401 USA.
RP Zhai, PW (reprint author), Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
EM pwzhai@umbc.edu
RI Hu, Yongxiang/K-4426-2012; Boss, Emmanuel/C-5765-2009; Franz,
Bryan/D-6284-2012
OI Boss, Emmanuel/0000-0002-8334-9595; Franz, Bryan/0000-0003-0293-2082
FU NASA Radiation Science program; Biology and Biogeochemistry program;
NASA grant, from NASA Biology and Biogeochemistry program [NNX15AC08G]
FX This study is partially supported by the NASA Radiation Science program
administrated Hal Maring and the Biology and Biogeochemistry program
administrated by Paula Bontempi. Peng-wang Zhai also thanks the PACE
science team for inspiring this work. Emmanuel Boss is funded by NASA
grant NNX15AC08G, from NASA Biology and Biogeochemistry program. We
thank Dr. Westberry for useful discussions about Raman scattering.
NR 48
TC 1
Z9 1
U1 1
U2 10
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 SEP 7
PY 2015
VL 23
IS 18
BP 23582
EP 23596
DI 10.1364/OE.23.023582
PG 15
WC Optics
SC Optics
GA CS9OG
UT WOS:000362419900055
PM 26368456
ER
PT J
AU Sarkhel, S
Mathews, JD
Raizada, S
Sekar, R
Chakrabarty, D
Guharay, A
Jee, G
Kim, JH
Kerr, RB
Ramkumar, G
Sridharan, S
Wu, Q
Mlynczak, MG
Russell, JM
AF Sarkhel, Sumanta
Mathews, John D.
Raizada, Shikha
Sekar, Ramanathan
Chakrabarty, Dibyendu
Guharay, Amitava
Jee, Geonhwa
Kim, Jeong-Han
Kerr, Robert B.
Ramkumar, Geetha
Sridharan, Sundararajan
Wu, Qian
Mlynczak, Martin G.
Russell, James M.
TI A case study on occurrence of an unusual structure in the sodium layer
over Gadanki, India (vol 67, 19, 2015)
SO EARTH PLANETS AND SPACE
LA English
DT Correction
C1 [Sarkhel, Sumanta; Mathews, John D.] Penn State Univ, Radar Space Sci Lab, University Pk, PA 16802 USA.
[Sarkhel, Sumanta; Raizada, Shikha; Kerr, Robert B.] SRI Int, Space & Atmospher Sci, Arecibo Observ, Ctr Geospace Studies, Arecibo, PR USA.
[Sarkhel, Sumanta; Jee, Geonhwa; Kim, Jeong-Han] Korea Polar Res Inst, Div Climate Change, Inchon 406840, South Korea.
[Sarkhel, Sumanta] Indian Inst Technol Roorkee, Dept Phys, Roorkee 247667, Uttar Pradesh, India.
[Sekar, Ramanathan; Chakrabarty, Dibyendu] Phys Res Lab, Space & Atmospher Sci Div, Ahmadabad 380009, Gujarat, India.
[Guharay, Amitava] Natl Inst Space Res, Sao Paulo, Brazil.
[Ramkumar, Geetha] Vikram Sarabhai Space Ctr, Space Phys Lab, Thiruvananthapuram, Kerala, India.
[Sridharan, Sundararajan] Natl Atmospher Res Lab, Gadanki, India.
[Wu, Qian] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Mlynczak, Martin G.] NASA, Langley Res Ctr, Div Atmospher Sci, Hampton, VA 23665 USA.
[Russell, James M.] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
RP Sarkhel, S (reprint author), Penn State Univ, Radar Space Sci Lab, 323 Elect Engn East, University Pk, PA 16802 USA.
EM sarkhel.fph@iitr.ac.in
NR 1
TC 1
Z9 1
U1 0
U2 0
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1880-5981
J9 EARTH PLANETS SPACE
JI Earth Planets Space
PD SEP 7
PY 2015
VL 67
AR 145
DI 10.1186/s40623-015-0276-1
PG 1
WC Geosciences, Multidisciplinary
SC Geology
GA CQ9MG
UT WOS:000360938500001
ER
PT J
AU Galetzka, J
Melgar, D
Genrich, JF
Geng, J
Owen, S
Lindsey, EO
Xu, X
Bock, Y
Avouac, JP
Adhikari, LB
Upreti, BN
Pratt-Sitaula, B
Bhattarai, TN
Sitaula, BP
Moore, A
Hudnut, KW
Szeliga, W
Normandeau, J
Fend, M
Flouzat, M
Bollinger, L
Shrestha, P
Koirala, B
Gautam, U
Bhatterai, M
Gupta, R
Kandel, T
Timsina, C
Sapkota, SN
Rajaure, S
Maharjan, N
AF Galetzka, J.
Melgar, D.
Genrich, J. F.
Geng, J.
Owen, S.
Lindsey, E. O.
Xu, X.
Bock, Y.
Avouac, J-P
Adhikari, L. B.
Upreti, B. N.
Pratt-Sitaula, B.
Bhattarai, T. N.
Sitaula, B. P.
Moore, A.
Hudnut, K. W.
Szeliga, W.
Normandeau, J.
Fend, M.
Flouzat, M.
Bollinger, L.
Shrestha, P.
Koirala, B.
Gautam, U.
Bhatterai, M.
Gupta, R.
Kandel, T.
Timsina, C.
Sapkota, S. N.
Rajaure, S.
Maharjan, N.
TI Slip pulse and resonance of the Kathmandu basin during the 2015 Gorkha
earthquake, Nepal
SO SCIENCE
LA English
DT Article
ID STRONG-MOTION; FRICTION LAWS; GROUND-MOTION; RUPTURE; HIMALAYA; GPS;
INVERSION; FAULTS; TIME
AB Detailed geodetic imaging of earthquake ruptures enhances our understanding of earthquake physics and associated ground shaking. The 25 April 2015 moment magnitude 7.8 earthquake in Gorkha, Nepal was the first large continental megathrust rupture to have occurred beneath a high-rate (5-hertz) Global Positioning System (GPS) network. We used GPS and interferometric synthetic aperture radar data to model the earthquake rupture as a slip pulse similar to 20 kilometers in width, similar to 6 seconds in duration, and with a peak sliding velocity of 1.1 meters per second, which propagated toward the Kathmandu basin at similar to 3.3 kilometers per second over similar to 140 kilometers. The smooth slip onset, indicating a large (similar to 5-meter) slip-weakening distance, caused moderate ground shaking at high frequencies (>1 hertz; peak ground acceleration, similar to 16% of Earth's gravity) and minimized damage to vernacular dwellings. Whole-basin resonance at a period of 4 to 5 seconds caused the collapse of tall structures, including cultural artifacts.
C1 [Galetzka, J.; Genrich, J. F.; Owen, S.; Avouac, J-P] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Melgar, D.] Univ Calif Berkeley, Berkeley Seismol Lab, Berkeley, CA 94720 USA.
[Geng, J.; Lindsey, E. O.; Xu, X.; Bock, Y.] Univ Calif San Diego, Scripps Inst Oceanog, Cecil H & Ida M Green Inst Geophys & Planetary Ph, La Jolla, CA 92037 USA.
[Moore, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Avouac, J-P] Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England.
[Adhikari, L. B.; Shrestha, P.; Koirala, B.; Gautam, U.; Bhatterai, M.; Gupta, R.; Kandel, T.; Timsina, C.; Sapkota, S. N.; Rajaure, S.; Maharjan, N.] Dept Mines & Geol, Kathmandu, Nepal.
[Upreti, B. N.] Nepal Acad Sci & Technol, Khumaltar, Lalitpur, Nepal.
[Pratt-Sitaula, B.] Cent Washington Univ, Dept Geol Sci, Ellensberg, WA 98926 USA.
[Bhattarai, T. N.; Sitaula, B. P.] Tribhuvan Univ, Kathmandu, Nepal.
[Hudnut, K. W.] US Geol Survey, Pasadena, CA 91106 USA.
[Szeliga, W.] CWU, Pacific Northwest Geodet Array, Ellensburg, WA 98926 USA.
[Szeliga, W.] CWU, Dept Geol Sci, Ellensburg, WA 98926 USA.
[Normandeau, J.; Fend, M.] UNAVCO, Boulder, CO 80301 USA.
[Flouzat, M.; Bollinger, L.] CEA, DASE, F-91297 Bruyeres Le Chatel, Arpajon, France.
RP Avouac, JP (reprint author), CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM avouac@gps.caltech.edu
RI Bollinger, Laurent/B-7636-2008; Avouac, Jean-Philippe/B-5699-2015;
Hudnut, Kenneth/B-1945-2009
OI Bollinger, Laurent/0000-0002-5116-860X; Avouac,
Jean-Philippe/0000-0002-3060-8442; Hudnut, Kenneth/0000-0002-3168-4797
FU Caltech; DASE; Gordon and Betty Moore Foundation [GBMF 423.01, GBMF
3024]; NSF [EAR-1345136]; United Nations Development Programme; Nepal
Academy for Science and Technology; NASA (USA); Department of Foreign
International Development (UK); NSF; NASA under NSF [EAR-1261833]; NASA
[NNX14AQ53G, NNX14AT33G]; Royal Society
FX The GPS data are available from the UNAVCO website. The InSAR data are
available at http://topex.ucsd.edu/nepal/. The Nepal Geodetic Array was
funded by Caltech and DASE (to J.-P.A.) and by the Gordon and Betty
Moore Foundation, through grant GBMF 423.01 to the Caltech Tectonics
Observatory; support was maintained by NSF grant EAR-1345136. A. Miner
and the Pacific Northwest Geodetic Array (PANGA) at CWU are thanked for
technical assistance with the construction and operation of the
Tribhuvan University (TU)-CWU network. Additional funding for the TU-CWU
network came from the United Nations Development Programme and the Nepal
Academy for Science and Technology. The high-rate data were recovered
thanks to (i) a rapid intervention funded by NASA (USA) and the
Department of Foreign International Development (UK) and (ii)
engineering services provided by UNAVCO via the GAGE (Geodesy Advancing
Geosciences and EarthScope) Facility, with support from NSF and NASA
under NSF Cooperative Agreement no. EAR-1261833. We also thank Trimble
Navigation and the Vaidya family for supporting the rapid response. The
accelerometer record at KATNP was provided by USGS. We thank A. Nathan
(U.S. Embassy in Kathmandu), S. Hough, D. Given, I. Flores, and J.
Luetgert for contributions to the installation of this station. Research
at UC-Berkeley was funded by the Gordon and Betty Moore Foundation
through grant GBMF 3024. A portion of this work was carried out at JPL
under a contract with the NASA. The GPS data were processed by the
Advanced Rapid Imaging and Analysis Center for Natural Hazards (JPL) and
the Scripps Orbit and Permanent Array Center. The effort at the Scripps
Institution of Oceanography was funded by NASA grants NNX14AQ53G and
NNX14AT33G. Advanced Land Observing Satellite-2 data were provided by
the Japan Aerospace Exploration Agency under investigations 1148 and
1413. J.-P.A. thanks the Royal Society for support. We thank D. Dreger
for discussion and W. Mooney for comments. J.-P.A led the study and
wrote the article. D.M. performed the kinematic modeling and wrote the
article. Y.B. supervised the high-rate data processing and wrote the
article. J.Ga. led the field operations. J.Ge. conducted the high-rate
data processing. S.O., A.M., W.S., and J.F.G. conducted the low-rate
data analysis to estimate coseismic offsets. E.O.L. and X.X. conducted
the InSAR data processing. L.B. helped to organize the field operations.
All other authors contributed to building and servicing the GPS stations
and to the post-earthquake data recovery. All authors edited the
article.
NR 31
TC 74
Z9 77
U1 8
U2 61
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD SEP 4
PY 2015
VL 349
IS 6252
BP 1091
EP 1095
DI 10.1126/science.aac6383
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CQ5FO
UT WOS:000360628900040
PM 26249228
ER
PT J
AU Koppelmans, V
Mulavara, AP
Yuan, P
Cassady, KE
Cooke, KA
Wood, SJ
Reuter-Lorenz, PA
De Dios, YE
Stepanyan, V
Szecsy, DL
Gadd, NE
Kofman, I
Scott, JM
Downs, ME
BIoomberg, JJ
Ploutz-Snyder, L
Seidler, RD
AF Koppelmans, Vincent
Mulavara, Ajitkumar P.
Yuan, Peng
Cassady, Kaitlin E.
Cooke, Katherine A.
Wood, Scott J.
Reuter-Lorenz, Patricia A.
De Dios, Yini E.
Stepanyan, Vahagn
Szecsy, Darcy L.
Gadd, Nichol E.
Kofman, Igor
Scott, Jessica M.
Downs, Meghan E.
BIoomberg, Jacob J.
Ploutz-Snyder, Lori
Seidler, Rachael D.
TI Exercise as potential countermeasure for the effects of 70 days of bed
rest on cognitive and sensorimotor performance
SO FRONTIERS IN SYSTEMS NEUROSCIENCE
LA English
DT Article
DE cognition; sensorimotor functioning; exercise; bed rest; microgravity;
spaceflight analog; longitudinal
ID BODY NEGATIVE-PRESSURE; HEAD-DOWN TILT; WEIGHTLESSNESS; SPACEFLIGHT;
BALANCE; TIME; GAIT; READAPTATION; ADAPTATION; TASK
AB Background: Spaceflight has been associated with changes in gait and balance; it is unclear whether it affects cognition. Head down tilt bed rest (HDBR) is a microgravity analog that mimics cephalad fluid shifts and body unloading. In consideration of astronaut's health and mission success, we investigated the effects of HDBR on cognition and sensorimotor function. Furthermore, we investigated if exercise mitigates any cognitive and sensorimotor sequelae of spaceflight.
Method: We conducted a 70-day six-degree HDBR study in 10 male subjects who were randomly assigned to a HDBR supine exercise or a HDBR control group. Cognitive measures (i.e., processing speed, manual dexterity, psychomotor speed, visual dependency, and 2D and 3D mental rotation) and sensorimotor performance (functional mobility (FMT) and balance performance) were collected at 12 and 8 days pre-HDBR, at 7, 50, and 70 days in HDBR, and at 8 and 12 days post-HDBR. Exercise comprised resistance training, and continuous and high-intensity interval aerobic exercise. We also repeatedly assessed an outside-of-bed rest control group to examine metric stability.
Results: Small practice effects were observed in the control group for some tasks; these were taken into account when analyzing effects of HDBR. No significant effects of HDBR on cognition were observed, although visual dependency during HDBR remained stable in HDBR controls whereas it decreased in HDBR exercise subjects. Furthermore, HDBR was associated with loss of FMT and standing balance performance, which were almost fully recovered 12 days post-HDBR. Aerobic and resistance exercise partially mitigated the effects of HDBR on FMT and accelerated the recovery time course post-HDBR.
Discussion: HDBR did not significantly affect cognitive performance but did adversely affect FMT and standing balance performance. Exercise had some protective effects on the deterioration and recovery of FMT.
C1 [Koppelmans, Vincent; Yuan, Peng; Cassady, Kaitlin E.; Cooke, Katherine A.; Seidler, Rachael D.] Univ Michigan, Sch Kinesiol, Ann Arbor, MI 48109 USA.
[Mulavara, Ajitkumar P.; Wood, Scott J.; BIoomberg, Jacob J.; Ploutz-Snyder, Lori] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Mulavara, Ajitkumar P.; Scott, Jessica M.; Ploutz-Snyder, Lori] Univ Space Res Assoc, Houston, TX USA.
[Seidler, Rachael D.] Univ Michigan, Dept Psychol, Ann Arbor, MI 48109 USA.
[Wood, Scott J.] Azusa Pacific Univ, Dept Psychol, Azusa, CA USA.
[Reuter-Lorenz, Patricia A.; Seidler, Rachael D.] Univ Michigan, Neurosci Program, Ann Arbor, MI 48109 USA.
[De Dios, Yini E.; Stepanyan, Vahagn; Gadd, Nichol E.; Kofman, Igor] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Szecsy, Darcy L.] Bast Technol, Houston, TX USA.
[Downs, Meghan E.] Univ Houston, Dept Hlth & Human Performance, Houston, TX USA.
[Seidler, Rachael D.] Univ Michigan, Inst Gerontol, Ann Arbor, MI 48109 USA.
RP Seidler, RD (reprint author), Univ Michigan, Sch Kinesiol, 401 Washtenaw Ave, Ann Arbor, MI 48109 USA.
EM rseidler@umich.edu
NR 53
TC 5
Z9 5
U1 3
U2 5
PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
SN 1662-5137
J9 FRONT SYST NEUROSCI
JI Front. Syst. Neurosci.
PD SEP 3
PY 2015
VL 9
AR 121
DI 10.3389/fnsys.2015.00121
PG 14
WC Neurosciences
SC Neurosciences & Neurology
GA CU9GF
UT WOS:000363851900001
PM 26388746
ER
PT J
AU Cord, AF
Seppelt, R
Turner, W
AF Cord, Anna F.
Seppelt, Ralf
Turner, Woody
TI Monitor ecosystem services from space
SO NATURE
LA English
DT Letter
C1 [Cord, Anna F.; Seppelt, Ralf] UFZ Helmholtz Ctr Environm Res, Leipzig, Germany.
[Turner, Woody] NASA, Washington, DC 20546 USA.
RP Cord, AF (reprint author), UFZ Helmholtz Ctr Environm Res, Leipzig, Germany.
EM ralf.seppelt@ufz.de
NR 2
TC 1
Z9 1
U1 6
U2 50
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 SEP 3
PY 2015
VL 525
IS 7567
BP 33
EP 33
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CQ4SE
UT WOS:000360594100012
PM 26333459
ER
PT J
AU Arora, N
Russell, RP
Strange, N
Ottesen, D
AF Arora, Nitin
Russell, Ryan P.
Strange, Nathan
Ottesen, David
TI Partial Derivatives of the Solution to the Lambert Boundary Value
Problem
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID GRAVITY-ASSIST TRAJECTORIES; AUTOMATED DESIGN; OPTIMIZATION; ALGORITHMS;
MISSIONS; FLYBY; MARS
AB Two methods for deriving first-order partial derivatives of the outputs with respect to the inputs of the Lambert boundary value problem are presented. The first method assumes the Lambert problem is solved via the universal vercosine formulation. Taking advantage of inherent symmetries and intermediate variables, the derivatives are expressed in a computationally efficient form. The typical added cost of computing these partials is found to be approximate to 15 to 35% of the Lambert computed cost. A second set of the same partial derivatives is derived from the fundamental perturbation matrix, also known as the state transition matrix of the Keplerian initial value problem. The equations are formulated in terms of Battin's partitions of the state transition matrix and its adjoint. This alternative approach works with any Lambert formulation, including one that solves a perturbed Lambert problem, subject to the availability of the associated state transition matrix. The analytic partial derivatives enable fast trajectory optimization formulations that implicitly enforce continuity constraints via embedded Lambert problems.
C1 [Arora, Nitin; Strange, Nathan] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA.
[Russell, Ryan P.; Ottesen, David] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA.
RP Arora, N (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA.
EM Nitin.Arora@jpl.nasa.gov; ryan.russell@utexas.edu;
Nathan.J.Strange@jpl.nasa.gov; DavidOttesen@utexas.edu
FU NASA
FX Part of this research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. Richard
Battin made many lasting contributions to the field of astrodynamics. In
particular, the authors are grateful for his inspiration on the topics
of Lambert's problem and the Keplerian fundamental perturbation
matrices.
NR 28
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 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD SEP
PY 2015
VL 38
IS 9
SI SI
BP 1563
EP 1572
DI 10.2514/1.G001030
PG 10
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA CS1LV
UT WOS:000361827900004
ER
PT J
AU Li, F
Choudhari, M
Chang, CL
Kimmel, R
Adamczak, D
Smith, M
AF Li, Fei
Choudhari, Meelan
Chang, Chau-Lyan
Kimmel, Roger
Adamczak, David
Smith, Mark
TI Transition Analysis for the Ascent Phase of HIFiRE-1 Flight Experiment
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID GROUND TEST
AB The HIFiRE-1 flight experiment provided a valuable database for boundary-layer transition over a 7deg half-angle, circular cone model from supersonic to hypersonic Mach numbers as well as a range of Reynolds numbers and angles of incidence. This paper reports the findings from a computational analysis of the measured in-flight transition behavior during the ascent phase. Given a nearly zero angle of attack, computations indicate that the most likely cause for transition during the flight window of 19 to 22.5s is the amplification of second-mode instabilities in the laminar boundary layer, except in the vicinity of the cone meridian, where a roughness element was placed midway along the length of the cone. The growth of first-mode instabilities is found to be weak at all trajectory points analyzed from the ascent phase. Based on the time histories of temperature and/or heat flux at transducer locations within the aft portion of the cone, the onset of transition across the aforementioned window is found to correlate with an average linear N-factor, based on parabolized stability equations, of approximately 13.3. For times less than approximately 18s into the flight, the peak amplification ratio for second-mode disturbances is too small to cause transition because of the lower Mach numbers at earlier times. Therefore, the observed transition at these times is attributed to an unknown physical mechanism that is potentially related to the step discontinuities in surface height near the changes in surface material.
C1 [Li, Fei; Choudhari, Meelan; Chang, Chau-Lyan] NASA, Langley Res Ctr, Computat AeroSci Branch, MS 128, Hampton, VA 23681 USA.
[Kimmel, Roger; Adamczak, David] US Air Force, Res Lab, Aerosp Syst Directorate, Wright Patterson AFB, OH 45433 USA.
[Smith, Mark] NASA, Armstrong Res Ctr, Aerodynam & Prop Branch, Edwards AFB, CA 93523 USA.
RP Li, F (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, MS 128, Hampton, VA 23681 USA.
RI Choudhari, Meelan/F-6080-2017
OI Choudhari, Meelan/0000-0001-9120-7362
NR 8
TC 3
Z9 3
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 SEP
PY 2015
VL 52
IS 5
BP 1283
EP 1293
DI 10.2514/1.A33258
PG 11
WC Engineering, Aerospace
SC Engineering
GA CS1RM
UT WOS:000361845400002
ER
PT J
AU Atkins, BM
Queen, EM
AF Atkins, Brad M.
Queen, Eric M.
TI Internal Moving Mass Actuator Control for Mars Entry Guidance
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID CONTROL-SYSTEM; SPACECRAFT
AB An internal moving mass actuator control system is proposed for angle-of-attack and sideslip-based Mars precision entry guidance. Internal moving mass actuators provide vehicle control moments without direct interaction with the external flowfield. This enables trajectory control without destabilization concerns associated with aerodynamic flap ablation and flowfield interaction for both flap and thruster control systems. Angle-of-attack and sideslip control is proposed as an alternative to bank angle guidance for decoupling range and crossrange control for improved precision entry guidance. A new variant of the Apollo Earth return terminal guidance algorithm is presented and used to provide closed-loop attitude commands. A linear-quadratic controller with integral error action is synthesized and tuned for a Mars Phoenix-sized entry vehicle with two internal moving mass actuators for guidance command tracking. Nonlinear simulation of the controller for the eight-degree-of-freedom system demonstrates precision guidance to the nominal trajectory and final target for offnominal initial entry conditions for the flight-path angle, range, cross range, speed, and attitude.
C1 [Atkins, Brad M.] Virginia Polytech Inst & State Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24061 USA.
[Queen, Eric M.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
RP Atkins, BM (reprint author), Virginia Polytech Inst & State Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24061 USA.
EM atkbr@vt.edu; eric.m.queen@nasa.gov
FU National Defense Science and Engineering Graduate Fellowship Program
FX The authors thank the National Defense Science and Engineering Graduate
Fellowship Program for the financial support of this research. The
authors also thank Robbie Robertson of Virginia Polytechnic Institute
and State University for his help with generating an AutoCAD model for
inertia properties of the entry capsule. The authors also thank Craig
Woolsey of Virginia Polytechnic Institute and State University for his
helpful input in data presentation and the revision of this paper.
NR 19
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U1 3
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 SEP
PY 2015
VL 52
IS 5
BP 1294
EP 1310
DI 10.2514/1.A32970
PG 17
WC Engineering, Aerospace
SC Engineering
GA CS1RM
UT WOS:000361845400003
ER
PT J
AU Perino, SV
Bayandor, J
Armand, SC
Samareh, JA
AF Perino, Scott V.
Bayandor, Javid
Armand, Sasan C.
Samareh, Jamshid A.
TI Structural Concept Study for Planetary Probes and Sample Return Vehicles
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID DESIGN; EARTH
AB A parametric structural investigation of a new atmospheric entry vehicle concept for future planetary probes and sample return vehicles was conducted. During launch and reentry, the vehicle may experience large structural loads. To enable rapid assessment of candidate vehicle configurations for different missions, a parametric structural dynamics analysis methodology was developed. The methodology generates finite-element models and enables rapid modification to all aspects of the models, including geometry, material properties, load and boundary conditions, mesh parameters, and analysis controls. Analyses including quasi-static inertial loading, vibration frequency response, acoustic loading, and reentry loading were conducted for the structural concept study. Several geometry, mass, and material parameters were varied from -50 to +50% of their baseline value and analyzed. A total of 136 analyses were conducted on 34 unique vehicle configurations. Of the parameters investigated, cone angle and vehicle diameter were found to be the most influential on the vehicle's mass and structural response. The highest stress observed was for an inertial launch analysis conducted on a -50% cone angle model, which had 2.7x the baseline stress and only 1.4x the baseline mass. This analysis methodology is shown to facilitate and expedite future planetary exploration mission analyses.
C1 [Perino, Scott V.; Bayandor, Javid] Virginia Polytech Inst & State Univ, Dept Mech Engn, Crashworthiness Aerosp Struct & Hybrids CRASH Lab, Blacksburg, VA 24061 USA.
[Armand, Sasan C.] NASA, Langley Res Ctr, Struct & Thermal Syst Branch, Hampton, VA 23681 USA.
[Samareh, Jamshid A.] NASA, Langley Res Ctr, Vehicle Anal Branch, Hampton, VA 23681 USA.
RP Perino, SV (reprint author), Virginia Polytech Inst & State Univ, Dept Mech Engn, Crashworthiness Aerosp Struct & Hybrids CRASH Lab, Blacksburg, VA 24061 USA.
FU NASA In-Space Propulsion Technology program; National Institute of
Aerospace; Aaron Horning of Analytical Mechanics Associates, Inc.
FX This project was funded by the NASA In-Space Propulsion Technology
program. Bo Walkley of the National Institute of Aerospace and Aaron
Horning of Analytical Mechanics Associates, Inc., provided extensive
support and collaborative assistance on this project.
NR 33
TC 0
Z9 0
U1 1
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP
PY 2015
VL 52
IS 5
BP 1320
EP 1330
DI 10.2514/1.A33050
PG 11
WC Engineering, Aerospace
SC Engineering
GA CS1RM
UT WOS:000361845400005
ER
PT J
AU Centinello, FJ
Zuber, MT
Smith, DE
Mazarico, E
AF Centinello, Frank J., III
Zuber, Maria T.
Smith, David E.
Mazarico, Erwan
TI Orbit Determination of the Dawn Spacecraft with Radiometric and Image
Data
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID LUNAR RECONNAISSANCE ORBITER; GRAVITY-FIELD; MISSION; EPHEMERIS;
MESSENGER; RECOVERY; MERCURY; MODELS; SYSTEM
AB The orbit of the Dawn spacecraft around asteroid 4 Vesta has been reconstructed using radiometric measurements and image control points. Image control points are introduced as a new measurement type because they constrain the orbit in the along- and crosstrack directions, whereas radiometric measurements provide a stronger constraint in the radial direction. Image control points are available whenever two image footprints on the surface overlap. The measurement uncertainty of images is limited by pixel scale that, in the case of the Dawn mission at Vesta, is between 20 and 150m/pixel. The obtained image constraint residual root mean square is approximately the pixel scale for all mission phases. Radiometric residual root mean square spanned from 0.07 to 0.44mm/s for Doppler and from 0.7 to 1.5m for range measurements. Radiometric and image constraint residual root-mean-square values are comparable to those reported by the Dawn Science Team using independent software and processing methodology. Improvements as a result of including image control points are largest in the along- and crosstrack directions during the survey phase of the mission. Agreement between the current orbit reconstruction and the trajectory archived by the Dawn Gravity Science Team improves from several kilometers with radiometric measurements to hundreds of meters when image control points are included.
C1 [Centinello, Frank J., III; Zuber, Maria T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Bldg 54-317,77 Massachusetts Avenue, Cambridge, MA 02139 USA.
[Mazarico, Erwan] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Centinello, FJ (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Bldg 54-317,77 Massachusetts Avenue, Cambridge, MA 02139 USA.
RI Mazarico, Erwan/N-6034-2014
OI Mazarico, Erwan/0000-0003-3456-427X
FU NASA Dawn Mission
FX This work would not have been possible without the support and advice
generously provided by Christopher T. Russell (University of California,
Los Angeles/Dawn), Carol Raymond [Jet Propulsion Laboratory (JPL)/Dawn],
Sami Asmar (JPL), Ryan Park (JPL), Alex Konopliv (JPL), Bob Gaskell
(Planetary Science Institute), Despina Pavlis (Stinger Ghaffarian
Technologies), Mark Torrance (Stinger Ghaffarian Technologies), David
Rowlands (Goddard Space Flight Center), Frank Lemoine (Goddard Space
Flight Center), and Anton Ermakov (Massachusetts Institute of
Technology). This work was supported by the NASA Dawn Mission.
NR 33
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U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP
PY 2015
VL 52
IS 5
BP 1331
EP 1337
DI 10.2514/1.A33224
PG 7
WC Engineering, Aerospace
SC Engineering
GA CS1RM
UT WOS:000361845400006
ER
PT J
AU Jesick, M
AF Jesick, Mark
TI Mars Double-Flyby Free Returns
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID EARTH; OPTIMIZATION; TRAJECTORIES; MISSION; ASSIST; CYCLER
AB A subset of Earth-originating Mars double-flyby ballistic trajectories is documented. The subset consists of those trajectories that, after the first Mars flyby, perform a half-revolution transfer with Mars before returning to Earth. This class of free returns is useful for both human and robotic Mars missions because of its low geocentric energy at departure and arrival, and because of its extended stay time in the vicinity of Mars. Ballistic opportunities are documented over Earth departure dates ranging from 2015 through 2100. The mission is viable over three or four consecutive Mars synodic periods and unavailable for the next four, with the pattern repeating approximately every 15 years. Over the remainder of the century, a minimum Earth departure hyperbolic excess speed of 3.16km/s, a minimum Earth atmospheric entry speed of 11.47km/s, and a minimum flight time of 904 days are observed. The algorithm used to construct these trajectories is presented along with several examples.
C1 [Jesick, Mark] CALTECH, Jet Prop Lab, Inner Planet Nav Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Jesick, M (reprint author), CALTECH, Jet Prop Lab, Inner Planet Nav Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jesick@jpl.nasa.gov
NR 22
TC 0
Z9 0
U1 2
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP
PY 2015
VL 52
IS 5
BP 1348
EP 1360
DI 10.2514/1.A33282
PG 13
WC Engineering, Aerospace
SC Engineering
GA CS1RM
UT WOS:000361845400008
ER
PT J
AU Chou, A
Schneider, SP
AF Chou, Amanda
Schneider, Steven P.
TI Measurements of Resonance in a Forward-Facing Cavity at Mach Six
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID NOSE CAVITY
AB An experimental study of the resonance of a cylindrical forward-facing cavity was conducted in a Mach 6 quiet-flow wind tunnel. The diameter of this cavity was fixed and the depth was varied in order to find the critical depth at which the cavity resonance became self-sustained. At Mach 6, this critical depth was 1.2 diameters deep, regardless of the freestream noise levels. For cavities deeper than 1.2 diameters, measurements of root-mean-square pressure fluctuations were orders of magnitude larger than those in shallower cavities. In quiet flow, this increase was about 2.5 orders of magnitude. In noisy flow, this increase was only about one order of magnitude. However, the magnitude of the pressure fluctuations within deep cavities was about the same in quiet flow as it was in noisy flow. The damping characteristics of a shallow cavity (depth less than 1.2 diameters) were also studied by observing the cavity response to a freestream laser-generated perturbation. The perturbation convects with the flow and interacts with the model's flowfield, causing pressure fluctuations in the forward-facing cavity. These pressure fluctuations damp exponentially in shallow cavities. The damping characteristics of such cavities appear to be related to the nondimensional cavity depth, regardless of stagnation pressure, stagnation temperature, and Mach number.
C1 [Chou, Amanda] NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23681 USA.
[Schneider, Steven P.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
RP Chou, A (reprint author), NASA, Langley Res Ctr, Flow Phys & Control Branch, Hampton, VA 23681 USA.
FU U.S. Air Force Office of Scientific Research [FA9550-12-1-0167];
National Defense Science & Engineering Graduate fellowship
FX This research was funded by U.S. Air Force Office of Scientific Research
grant FA9550-12-1-0167 and a National Defense Science & Engineering
Graduate fellowship. The authors would like to thank Jerry Hahn, Jim
Younts, and Robin Snodgrass for their quality craftsmanship. The optical
system for the laser perturber was designed by Steven H. Collicott. The
forward-facing cavity model was designed by Rodrigo Segura.
NR 23
TC 2
Z9 2
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 SEP
PY 2015
VL 52
IS 5
BP 1486
EP 1494
DI 10.2514/1.A33286
PG 9
WC Engineering, Aerospace
SC Engineering
GA CS1RM
UT WOS:000361845400020
ER
PT J
AU Donnellan, A
Ludwig, LG
Parker, JW
Rundle, JB
Wang, J
Pierce, M
Blewitt, G
Hensley, S
AF Donnellan, Andrea
Ludwig, Lisa Grant
Parker, Jay W.
Rundle, John B.
Wang, Jun
Pierce, Marlon
Blewitt, Geoffrey
Hensley, Scott
TI Potential for a large earthquake near Los Angeles inferred from the 2014
La Habra earthquake
SO EARTH AND SPACE SCIENCE
LA English
DT Article
ID SAN-ANDREAS FAULT; BLIND-THRUST-FAULT; TRANSVERSE RANGES; THRESHOLD
SYSTEMS; STRIKE-SLIP; CALIFORNIA; DEFORMATION; TECTONICS; DYNAMICS;
BASIN
AB Tectonic motion across the Los Angeles region is distributed across an intricate network of strike-slip and thrust faults that will be released in destructive earthquakes similar to or larger than the 1933M6.4 Long Beach and 1994M6.7 Northridge events. Here we show that Los Angeles regional thrust, strike-slip, and oblique faults are connected and move concurrently with measurable surface deformation, even in moderate magnitude earthquakes, as part of a fault system that accommodates north-south shortening and westerly tectonic escape of northern Los Angeles. The 28 March 2014 M5.1 La Habra earthquake occurred on a northeast striking, northwest dipping left-lateral oblique thrust fault northeast of Los Angeles. We present crustal deformation observation spanning the earthquake showing that concurrent deformation occurred on several structures in the shallow crust. The seismic moment of the earthquake is 82% of the total geodetic moment released. Slip within the unconsolidated upper sedimentary layer may reflect shallow release of accumulated strain on still-locked deeper structures. A future M6.1-6.3 earthquake would account for the accumulated strain. Such an event could occur on any one or several of these faults, which may not have been identified by geologic surface mapping.
C1 [Donnellan, Andrea; Parker, Jay W.; Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Donnellan, Andrea] Univ So Calif, Dept Earth Sci, Loa Angeles, CA USA.
[Ludwig, Lisa Grant] Univ Calif Irvine, Program Publ Hlth, Irvine, CA USA.
[Rundle, John B.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Rundle, John B.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA.
[Wang, Jun; Pierce, Marlon] Indiana Univ, Univ Informat Technol Serv, Bloomington, IN USA.
[Blewitt, Geoffrey] Univ Nevada, Nevada Bur Mines & Geol, Nevada Geodet Lab, Reno, NV 89557 USA.
RP Donnellan, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM andrea.donnellan@jpl.nasa.gov
RI Ludwig, Lisa Grant/G-6442-2012
OI Ludwig, Lisa Grant/0000-0001-6538-8067
NR 33
TC 3
Z9 3
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2333-5084
J9 Earth Space Sci
JI Earth Space Sci.
PD SEP
PY 2015
VL 2
IS 9
BP 378
EP 385
DI 10.1002/2015EA000113
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DE6NL
UT WOS:000370750500002
PM 27981074
ER
PT J
AU Bedsole, RW
Park, C
Bogert, PB
Tippur, HV
AF Bedsole, Robert W.
Park, Cheol
Bogert, Philip B.
Tippur, Hareesh V.
TI A critical evaluation of the enhancement of mechanical properties of
epoxy modified using CNTs
SO MATERIALS RESEARCH EXPRESS
LA English
DT Article
DE carbon nanotubes; epoxy; mechanical properties; fracture toughness;
sonication; homogenization; calendering
ID CARBON NANOTUBE/EPOXY COMPOSITES; FRACTURE-TOUGHNESS; NANOCOMPOSITES;
TEMPERATURE; DISPERSION; RESINS
AB Carbon nanotubes (CNTs) have been widely shown in the literature to improve mechanical properties of epoxy, such as tensile strength, elastic modulus, strain to failure, and fracture toughness. These improvements in nanocomposite properties have been attributed to the extraordinary properties of the nanotubes, as well as the quality of their dispersion within and adhesion to the epoxy matrix. However, many authors have also struggled to show significant mechanical improvements using similar methodologies and despite, in some cases, showing qualitative improvements in dispersion with optical microscopy. These authors have frequently resorted to other methods for improving the mechanical properties of CNT/epoxy, such as electrically aligning CNTs, using different types of CNTs, or modifying the stoichiometry. The current work examines many different dispersion techniques, types of CNTs, types of epoxies, curing cycles, and other variables in an attempt to improve the mechanical properties of neat epoxy with CNTs. Despite seeing significant changes in the microscopy, no significant improvements in tensile or fracture properties have been attributed to CNTs in this work.
C1 [Bedsole, Robert W.; Tippur, Hareesh V.] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
[Park, Cheol] NASA, Adv Mat & Proc, LaRC, Hampton, VA 23681 USA.
[Bogert, Philip B.] NASA, Struct Mech & Concepts, LaRC, Hampton, VA 23681 USA.
RP Bedsole, RW (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
EM tippuhv@auburn.edu
FU NASA Office of the Chief Technologist's Space Technology Research
Fellowship (NSTRF)
FX This work was supported by a NASA Office of the Chief Technologist's
Space Technology Research Fellowship (NSTRF). Technical assistance of
Drs S Chu, J Hinkley, C Fay, L Gibbons, T Hou, S Lowther, J Smith, Mr J
Hocker, Mr S Britton, Mr R Chattin, Mr R Martin of NASA Langley Research
Center, Drs L Payton, M Auad, Mr I Marcell, Mr C Wortman, Mr D Sherer,
Mr S Moore, Ms M Sullivan, Mr B Sibaja of Auburn University, and Drs M
Hosur, A Tcherbi-Narteh, E Triggs, Mr M Davis of Tuskegee University is
gratefully acknowledged. Special thanks to Bayer Ag and Momentive
Specialty Chemicals, Inc. for providing carbon nanotubes and epoxy,
respectively, for this investigation.
NR 32
TC 1
Z9 1
U1 1
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2053-1591
J9 MATER RES EXPRESS
JI Mater. Res. Express
PD SEP
PY 2015
VL 2
IS 9
AR 095020
DI 10.1088/2053-1591/2/9/095020
PG 23
WC Materials Science, Multidisciplinary
SC Materials Science
GA DD6TK
UT WOS:000370057200020
ER
PT J
AU Brown, ST
Kunkee, DB
AF Brown, Shannon T.
Kunkee, David B.
TI Foreword to the Special Issue on the 13th Specialist Meeting on
Microwave Radiometry and Remote Sensing of the Environment (MicroRad
2014)
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Editorial Material
C1 [Brown, Shannon T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kunkee, David B.] Aerosp Corp, Radar & Signal Syst Dept, Los Angeles, CA 90009 USA.
RP Brown, ST (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 0
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 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD SEP
PY 2015
VL 8
IS 9
SI SI
BP 1
EP 2
DI 10.1109/JSTARS.2015.2508518
PG 2
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA CZ8AW
UT WOS:000367323300001
ER
PT J
AU Draper, DW
Newell, DA
McKague, DS
Piepmeier, JR
AF Draper, David W.
Newell, David A.
McKague, Darren S.
Piepmeier, Jeffrey R.
TI Assessing Calibration Stability Using the Global Precipitation
Measurement (GPM) Microwave Imager (GMI) Noise Diodes
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article; Proceedings Paper
CT 13th Specialist Meeting on Microwave Radiometry and Remote Sensing of
the Environment (MicroRad)
CY MAR 24-27, 2014
CL Pasadena, CA
SP Inst Elect & Elect Engineers, IEEE Geoscience & Remote Sensing Soc
DE Calibration; microwave radiometry; noise diodes
AB With rising demand for smaller, lower mass microwave instruments, internal calibration using noise diodes is becoming increasingly more attractive for space-borne radiometer applications. Since noise diodes can exhibit on-orbit excess temperature drift, internally calibrated systems typically require vicarious on-orbit recharacterization. The GMI is the first instrument of its kind to include both internal (noise diodes) and external (hot load/cold sky) calibration systems. The dual-calibration system provides the unprecedented capability to directly measure transient behaviors in the hot load, cold sky view, and receiver nonlinearity. Furthermore, the behavior of the noise diodes can be directly evaluated, which may shed light on improvements to internal calibration for future missions. This paper directly examines the behavior of the GMI noise diodes using the hot load and cold sky views for the first 6 months of operations. Two of the seven channels with noise diodes have exhibited on-orbit noise diode excess temperature drift of about 1 K. The other noise diodes have remained exceptionally stable. The noise diodes are used to evaluate transient behaviors in the GMI hot load, cold sky view, and nonlinearity. The hot-load brightness temperature variation due to gradients is re-evaluated and shown to be smaller at the lower frequencies than at preflight calibration. Radio frequency interference (RFI) in the cold view is evaluated using the noise diode backup calibration. The on-orbit nonlinearity is trended over the first 6 months and shown to be stable over that time period.
C1 [Draper, David W.; Newell, David A.] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA.
[McKague, Darren S.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Piepmeier, Jeffrey R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Draper, DW (reprint author), Ball Aerosp & Technol Corp, Boulder, CO 80301 USA.
EM ddraper@ball.com; dnewell@ball.com; dmckague@umich.edu;
jeffrey.r.piepmeier@nasa.gov
RI Measurement, Global/C-4698-2015; McKague, Darren/J-2590-2012
OI McKague, Darren/0000-0003-0297-0388
FU Goddard Space Flight Center GPM program
FX This work was supported by the Goddard Space Flight Center GPM program.
NR 11
TC 6
Z9 6
U1 2
U2 3
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 SEP
PY 2015
VL 8
IS 9
SI SI
BP 4239
EP 4247
DI 10.1109/JSTARS.2015.2406661
PG 9
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA CZ8AW
UT WOS:000367323300003
ER
PT J
AU Yanovsky, I
Lambrigtsen, BH
Tanner, AB
Vese, LA
AF Yanovsky, Igor
Lambrigtsen, Bjorn H.
Tanner, Alan B.
Vese, Luminita A.
TI Efficient Deconvolution and Super-Resolution Methods in Microwave
Imagery
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article; Proceedings Paper
CT 13th Specialist Meeting on Microwave Radiometry and Remote Sensing of
the Environment (MicroRad)
CY MAR 24-27, 2014
CL Pasadena, CA
SP Inst Elect & Elect Engineers, IEEE Geoscience & Remote Sensing Soc
DE Aperture synthesis system; inverse problems; microwave imaging; remote
sensing; sparse optimization; spatial resolution; super-resolution
ID RESTORATION; REGULARIZATION; ALGORITHMS; RECONSTRUCTION; MINIMIZATION;
RADIOMETER; NOISE; TV
AB In this paper, we develop efficient deconvolution and super-resolution methodologies, and apply these techniques to reduce image blurring and distortion inherent in an aperture synthesis system. Such a system produces ringing at sharp edges and other transitions in the observed field. The conventional approach to suppressing sidelobes is to apply linear apodization, which has the undesirable side effect of degrading spatial resolution. We have developed an efficient total variation minimization technique based on Split Bregman deconvolution that reduces image ringing while sharpening the image and preserving information content. The model was generalized to include upsampling of deconvolved images to a higher resolution grid. Furthermore, a proposed multi-frame super-resolution method is presented that is robust to image noise and noise in the point spread function, and leads to additional improvements in spatial resolution. Our super-resolution methodologies are based on current research in sparse optimization and compressed sensing, which lead to unprecedented efficiencies for solving image reconstruction problems.
C1 [Yanovsky, Igor; Lambrigtsen, Bjorn H.; Tanner, Alan B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Yanovsky, Igor] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Vese, Luminita A.] Univ Calif Los Angeles, Dept Math, Los Angeles, CA 90095 USA.
RP Yanovsky, I (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM igor.yanovsky@jpl.nasa.gov
FU National Science Foundation [DMS 1217239]
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. The work of I. Yanovsky and L. A. Vese was
also supported by the National Science Foundation under Grant DMS
1217239.
NR 32
TC 4
Z9 4
U1 2
U2 8
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 SEP
PY 2015
VL 8
IS 9
SI SI
BP 4273
EP 4283
DI 10.1109/JSTARS.2015.2424451
PG 11
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA CZ8AW
UT WOS:000367323300006
ER
PT J
AU Islam, T
Rico-Ramirez, MA
Srivastava, PK
Dai, Q
Han, DW
Gupta, M
Zhuo, L
AF Islam, Tanvir
Rico-Ramirez, Miguel A.
Srivastava, Prashant K.
Dai, Qiang
Han, Dawei
Gupta, Manika
Zhuo, Lu
TI CLOUDET: A Cloud Detection and Estimation Algorithm for Passive
Microwave Imagers and Sounders Aided by Naive Bayes Classifier and
Multilayer Perceptron
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article; Proceedings Paper
CT 13th Specialist Meeting on Microwave Radiometry and Remote Sensing of
the Environment (MicroRad)
CY MAR 24-27, 2014
CL Pasadena, CA
SP Inst Elect & Elect Engineers, IEEE Geoscience & Remote Sensing Soc
DE Cloud classification and masking; cloud liquid water path; hydrometeor
retrieval algorithm; passive microwave remote sensing; rain water path;
special sensor microwave imager/sounder (SSMIS)
ID PERFORMANCE; RADAR
AB CLOUDET, a cloud detection and estimation algorithm for passive microwave imagers and sounders is presented. CLOUDET is based on a naive Bayes classifier and multilayer perceptron. It is applied to the special sensor microwave imager/sounder (SSMIS), and the ECMWF integrated forecast system (IFS) cloud liquid water information has been used to train the algorithm. CLOUDET is applicable to both ocean and land-surface types. CLOUDET has been developed and evaluated by employing two different groups of radiometric information, namely, the humidity channels near 183 GHz (humidity algorithm) and the window channels between 19 and 91 GHz (window algorithm). It has been revealed that both humidity and window algorithms can detect cloudy scenes over ocean at a confidence level of more than 90% (80% over land). The analysis indicates that the humidity algorithm has a better ability in detecting cloudy scenes over ocean than the window algorithm (vs.). The (CSI = 0.98 vs. CSI = 0.93) opposite is true over land-surface type, revealing a CSI of 0.85 by humidity algorithm as opposed to CSI of 0.88 by window algorithm. The estimation of cloud by the CLOUDET algorithm has also been very promising during the validation effort. In particular, the correlation coefficient obtained over ocean through the use of the window algorithm is 0.70 (MAE 0.04 mm and RMSE 0.09 mm). The presented algorithm CLOUDET can be served as a stand-alone tool to reject and identify the cloudy scenes as well as to estimate the cloud liquid water path amount prior to assimilating the radiances into numerical weather prediction model.
C1 [Islam, Tanvir] NOAA, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res STAR, College Pk, MD 20740 USA.
[Islam, Tanvir] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Islam, Tanvir; Rico-Ramirez, Miguel A.; Srivastava, Prashant K.; Dai, Qiang; Han, Dawei; Zhuo, Lu] Univ Bristol, Dept Civil Engn, Bristol BS8 1TR, Avon, England.
[Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Gupta, Manika] Indian Inst Technol Delhi, Dept Civil Engn, New Delhi 110016, India.
RP Islam, T (reprint author), NOAA, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res STAR, College Pk, MD 20740 USA.
EM tanvir.islam@noaa.gov
RI Rico-Ramirez, Miguel/H-3248-2014;
OI Rico-Ramirez, Miguel/0000-0002-8885-4582; Islam,
Tanvir/0000-0003-2429-3074
NR 17
TC 2
Z9 2
U1 1
U2 5
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 SEP
PY 2015
VL 8
IS 9
SI SI
BP 4296
EP 4301
DI 10.1109/JSTARS.2014.2321559
PG 6
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA CZ8AW
UT WOS:000367323300008
ER
PT J
AU Srivastava, PK
O'Neill, P
Cosh, M
Kurum, M
Lang, R
Joseph, A
AF Srivastava, Prashant K.
O'Neill, Peggy
Cosh, Michael
Kurum, Mehmet
Lang, Roger
Joseph, Alicia
TI Evaluation of Dielectric Mixing Models for Passive Microwave Soil
Moisture Retrieval Using Data From ComRAD Ground-Based SMAP Simulator
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article; Proceedings Paper
CT 13th Specialist Meeting on Microwave Radiometry and Remote Sensing of
the Environment (MicroRad)
CY MAR 24-27, 2014
CL Pasadena, CA
SP Inst Elect & Elect Engineers, IEEE Geoscience & Remote Sensing Soc
DE Combined radar/radiometer (ComRAD); dielectric models; L band;
single-channel algorithm (SCA); soil moisture
ID SOUTHERN GREAT-PLAINS; SURFACE-ROUGHNESS; SMOS SATELLITE; WATER-CONTENT;
WET SOIL; RADIOMETRY; EMISSION; BEHAVIOR; MISSION; RADAR
AB Soil moisture measurements are required to improve our understanding of hydrological processes and linkages between the Earth's water, energy, and carbon cycles. The efficient retrieval of soil moisture depends on various factors among which soil dielectric mixing models are considered to be an important factor. The main objective of this work focuses on testing different dielectric models-Mironov et al., Dobson et al., Wang and Schmugge, and Hallikainen et al.-for soil moisture retrieval using the combined radar/radiometer (ComRAD) ground-based L-band simulator system, which serves as a simulator for the instruments on NASA's soil moisture active passive (SMAP) mission scheduled for launch in early next year. The single-channel algorithm at H polarization (SCA-H) version of the tau-omega model was used for soil moisture retrieval. A summer field experiment was conducted in 2012 at the United States Department of Agriculture (USDA) test site from which ComRAD measurements and validation samples of soil moisture were collected using theta probes and in situ sensors. The highest performance statistics combination in terms of high correlation (r), low root-mean-square error (RMSE), and least bias has been obtained with SCA-H using the Mironov dielectric model (r = 0.79; RMSE = 0.04 m(3)/m(3); bias = 0.01) followed by Dobson (r = 0.76; RMSE = 0.04 m(3)/m(3), bias = -0.01), Wang and Schmugge (r = 0.79; RMSE = 0.04 m(3)/m(3), bias = 0.02) and Hallikainen (r = 0.76; RMSE = 0.06 m(3)/m(3), bias = 0.04). Although the performance of the four dielectric models is relatively comparable, this analysis indicates that the Mironov dielectric model is marginally better than others for passive-only microwave soil moisture retrieval and could be a useful choice for SMAP satellite soil moisture retrieval.
C1 [Srivastava, Prashant K.; O'Neill, Peggy; Joseph, Alicia] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Cosh, Michael] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Kurum, Mehmet] TUBITAK BILGEM, Inst Informat Technol, TR-41470 Gebze, Kocaeli, Turkey.
[Lang, Roger] George Washington Univ, Dept Elect & Comp Engn, Washington, DC 20052 USA.
RP Srivastava, PK (reprint author), NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
OI Cosh, Michael/0000-0003-4776-1918
NR 42
TC 2
Z9 2
U1 7
U2 13
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 SEP
PY 2015
VL 8
IS 9
SI SI
BP 4345
EP 4354
DI 10.1109/JSTARS.2014.2372031
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 CZ8AW
UT WOS:000367323300013
ER
PT J
AU Forman, BA
Reichle, RH
AF Forman, Barton A.
Reichle, Rolf H.
TI Using a Support Vector Machine and a Land Surface Model to Estimate
Large-Scale Passive Microwave Brightness Temperatures Over Snow-Covered
Land in North America
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article; Proceedings Paper
CT 13th Specialist Meeting on Microwave Radiometry and Remote Sensing of
the Environment (MicroRad)
CY MAR 24-27, 2014
CL Pasadena, CA
SP Inst Elect & Elect Engineers, IEEE Geoscience & Remote Sensing Soc
DE Advanced microwave scanning radiometer (AMSR-E); brightness temperature;
land assimilation; modeling; passive microwave (PMW); remote sensing;
snow; support vector machines (SVMs)
ID WATER EQUIVALENT; NEURAL-NETWORK; RADIOMETER DATA; AMSR-E; REGRESSION;
CLIMATE; ASSIMILATION; UNCERTAINTY; PERFORMANCE; PARAMETERS
AB A support vector machine (SVM), a machine learning technique developed from statistical learning theory, is employed for the purpose of estimating passive microwave (PMW) brightness temperatures over snow-covered land in North America as observed by the advanced microwave scanning radiometer (AMSR-E) satellite sensor. The capability of the trained SVM is compared relative to the artificial neural network (ANN) estimates originally presented in [ 16]. The results suggest that the SVM outperforms the ANN at 10.65, 18.7, and 36.5 GHz for both vertically and horizontally polarized PMW radiation. When compared against daily AMSR-E measurements not used during the training procedure and subsequently averaged across the North American domain over the 9-year study period, the root-mean-squared error (RMSE) in the SVM output is 8 K or less, while the anomaly correlation coefficient is 0.7 or greater. When compared relative to the results from the ANN at any of the six frequency and polarization combinations tested, the RMSE was reduced by more than 18%, while the anomaly correlation coefficient was increased by more than 52%. Furthermore, the temporal and spatial variability in the modeled brightness temperatures via the SVM more closely agrees with that found in the original AMSR-E measurements. These findings suggest that the SVM is a superior alternative to the ANN for eventual use as a measurement operator within a data assimilation framework.
C1 [Forman, Barton A.] Univ Maryland, Dept Civil & Environm Engn, College Pk, MD 20742 USA.
[Reichle, Rolf H.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Forman, BA (reprint author), Univ Maryland, Dept Civil & Environm Engn, College Pk, MD 20742 USA.
EM baforman@umd.edu
RI Reichle, Rolf/E-1419-2012
FU Minta Martin Foundation; NASA
FX The work of B. A. Forman was supported by the Minta Martin Foundation.
The work of R. H. Reichle was supported by the NASA program on the
Science of Terra and Aqua.
NR 45
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Z9 2
U1 1
U2 5
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 SEP
PY 2015
VL 8
IS 9
SI SI
BP 4431
EP 4441
DI 10.1109/JSTARS.2014.2325780
PG 11
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA CZ8AW
UT WOS:000367323300020
ER
PT J
AU Roy, A
Royer, A
Derksen, C
Brucker, L
Langlois, A
Mialon, A
Kerr, YH
AF Roy, Alexandre
Royer, Alain
Derksen, Chris
Brucker, Ludovic
Langlois, Alexandre
Mialon, Arnaud
Kerr, Yann H.
TI Evaluation of Spaceborne L-Band Radiometer Measurements for Terrestrial
Freeze/Thaw Retrievals in Canada
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article; Proceedings Paper
CT 13th Specialist Meeting on Microwave Radiometry and Remote Sensing of
the Environment (MicroRad)
CY MAR 24-27, 2014
CL Pasadena, CA
SP Inst Elect & Elect Engineers, IEEE Geoscience & Remote Sensing Soc
DE Aquarius; Canada; freeze/thaw; passive microwave; polarization ratio;
SMOS
ID MICROWAVE EMISSION; RADIOMETER/SCATTEROMETER OBSERVATIONS; SALINITY
RETRIEVALS; OCEAN SALINITY; POLAR-REGIONS; DATA SETS; BOREAL; SOIL;
MODEL; SNOW
AB The landscape freeze/thaw (F/T) state has an important impact on the surface energy balance, carbon fluxes, and hydrologic processes; the timing of spring melt is linked to active layer dynamics in permafrost areas. L-band (1.4 GHz) microwave emission could allow the monitoring of surface state dynamics due to its sensitivity to the pronounced permittivity difference between frozen and thawed soil. The aim of this paper is to evaluate the performance of both Aquarius and soil moisture and ocean salinity (SMOS) L-band passive microwave measurements using a polarization ratio (PR)-based algorithm for landscape F/T monitoring. Weekly L-band satellite observations are compared with a large set of reference data at 48 sites across Canada spanning three environments: 1) tundra; 2) boreal forest; and 3) prairies. The reference data include in situ measurements of soil temperature (T-soil) and air temperature (T-air), and moderate resolution imaging spectroradiometer (MODIS) land surface temperature (LST) and snow cover area (SCA) products. Results show generally good agreement between L-band F/T detection and the surface state estimated from four reference datasets. The best apparent accuracies for all seasons are obtained using T-air as the reference. Aquarius radiometer 2 (incidence angle of 39.6 degrees) data give the best accuracies (90.8%), while for SMOS, using the Aquarius temporal characteristics, the best results (87.8% of accuracy) are obtained at higher incidence angles (55 degrees-60 degrees). The F/T algorithm identifies both freeze onset and end with a delay of about 1 week in tundra and 2 weeks in forest and prairies, when compared to T-air. The analysis shows a stronger F/T signal at tundra sites due to the typically clean transitions between consistently frozen and thawed conditions (and vice versa) and the absence of surface vegetation. Results in the prairies were poorer because of the influence of vegetation growth in summer (which decreases the PR) and the high frequency of ephemeral thaw events during winter. Freeze onset and end maps created from the same algorithm applied to SMOS and Aquarius measurements characterize similar F/T patterns over Canada. This study shows the potential of using L-band spaceborne observations for F/T monitoring, but underlines some limitations due to ice crusts in the snowpack, liquid water content in snow cover during the spring freeze to thaw transition, and vegetation growth.
C1 [Roy, Alexandre; Royer, Alain; Langlois, Alexandre] Univ Sherbrooke, Ctr Applicat & Rech Teledetect CARTEL, Sherbrooke, PQ J1K 2R1, Canada.
[Roy, Alexandre; Derksen, Chris] Environm Canada, Div Climate Res, Toronto, ON M3H 5T4, Canada.
[Brucker, Ludovic] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
[Brucker, Ludovic] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Columbia, MD 21044 USA.
[Mialon, Arnaud; Kerr, Yann H.] CNRS, IRD UT3, CESBIO CNES, F-31401 Toulouse, France.
RP Roy, A (reprint author), Univ Sherbrooke, Ctr Applicat & Rech Teledetect CARTEL, Sherbrooke, PQ J1K 2R1, Canada.
EM Alexandre.R.Roy@USherbrooke.ca
RI Brucker, Ludovic/A-8029-2010
OI Brucker, Ludovic/0000-0001-7102-8084
FU Canadian Space Agency (CSA) under the SMAP-Canada project; National
Sciences and Engineering Research Council of Canada (NSERC); Environment
Canada-Climate Research Division
FX This work was supported in part by the Canadian Space Agency (CSA) under
the SMAP-Canada project, in part by the National Sciences and
Engineering Research Council of Canada (NSERC), and in part by the and
Environment Canada-Climate Research Division.
NR 46
TC 6
Z9 6
U1 3
U2 11
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 SEP
PY 2015
VL 8
IS 9
SI SI
BP 4442
EP 4459
DI 10.1109/JSTARS.2015.2476358
PG 18
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA CZ8AW
UT WOS:000367323300021
ER
PT J
AU Chen, S
Hu, JJ
Zhang, ZX
Behrangi, A
Hong, Y
Gebregiorgis, AS
Cao, JR
Hu, BQ
Xue, XW
Zhang, XH
AF Chen, Sheng
Hu, Junjun
Zhang, Zengxin
Behrangi, Ali
Hong, Yang
Gebregiorgis, Abebe S.
Cao, Jianrong
Hu, Baoqing
Xue, Xianwu
Zhang, Xinhua
TI Hydrologic Evaluation of the TRMM Multisatellite Precipitation Analysis
Over Ganjiang Basin in Humid Southeastern China
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Hydrology; quantitative precipitation estimation; remote sensing;
satellite
ID PASSIVE-MICROWAVE; WATER-RESOURCES; ANALYSIS TMPA; LAND-SURFACE; POYANG
LAKE; REAL-TIME; RAINFALL; MODEL; PRODUCTS; PREDICTION
AB This study assesses the successive Version-6 and Version-7 TRMM Multisatellite Precipitation Analysis (TMPA) products including near-real-time products (3B42RTV6 and 3B42RTV7) and post-real-time research products (3B42V6 and 3B42V7) from March 2002 to February 2008 over Ganjiang Basin in the humid southeastern China, located in the lower reach of Yangtze River. Direct comparison of TMPA rainfall estimates with ground observation shows that the spatial and temporal rainfall characteristics over this region are well captured by 3B42V6, 3B42RTV7, and 3B42V7. In terms of daily grid-based comparison, 3B42RTV7 has been improved over 3B42RTV6 by reducing relative bias (RB) from-30.25% to 4.93%; 3B42V6, 3B42RTV7, and 3B42V7 show close performance with each other with RB less than 5% and moderate correlative coefficient (CC, 0.59). Daily hydrologic simulation with Xin'anjiang hydrologic model using these TMPA products as input shows that: 1) 3B42V6 and 3B42V7 demonstrate very comparable hydrologic skills, which are close to those of the reference rainfall with high Nash-Sutcliffe index (NSCE, 0.71 and 0.72, respectively) and strong correlation (CC = 0.88); and 2) 3B42RTV7 displays a better hydrologic performance than 3B42RTV6 by increasing the NSCE from 0.56 to 0.59, improving CC from 0.81 to 0.87, and reducing RB from -33.15% to 20.93%. This improvement of real-time TMPA product shows its potential hydrologic utility in water resource management and flood forecast. Finally, this study provides useful reference for TMPA developers and insights for the end users in their applications.
C1 [Chen, Sheng; Hu, Baoqing] Guangxi Teachers Educ Univ, Minist Educ, Key Lab Beibu Gulf Environm Evolut & Resources Ut, Nanning 530001, Peoples R China.
[Chen, Sheng; Hong, Yang; Gebregiorgis, Abebe S.; Xue, Xianwu] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA.
[Hu, Junjun] Univ Oklahoma, Sch Comp Sci, Norman, OK 73072 USA.
[Zhang, Zengxin] Nanjing Forestry Univ, Coll Biol & Environm, Joint Innovat Ctr Modern Forestry Studies, Nanjing 210037, Jiangsu, Peoples R China.
[Behrangi, Ali] CALTECH, Jet Prop Labs, Pasadena, CA 91109 USA.
[Hong, Yang; Gebregiorgis, Abebe S.; Xue, Xianwu] Univ Oklahoma, Adv Radar Res Ctr, Norman, OK 73019 USA.
[Cao, Jianrong] Liaocheng Univ, Coll Environm & Planning, Liaocheng 252059, Peoples R China.
[Zhang, Xinhua] Sichuan Univ, State Key Lab Hydraul & Mt River Engn, Chengdu 610065, Peoples R China.
RP Cao, JR (reprint author), Liaocheng Univ, Coll Environm & Planning, Liaocheng 252059, Peoples R China.
EM chenshengbj@gmail.com; caojianrong@lcu.edu.cn; xhzhang@scu.edu.cn
RI Gebregiorgis, Abebe/C-7947-2016; Hong, Yang/D-5132-2009
OI Gebregiorgis, Abebe/0000-0002-2975-9104; Hong, Yang/0000-0001-8720-242X
FU Natural Science Foundation of China [41361022, 41171020]; Guangxi
Science and Technology Development Project [2014DD29090]; Natural
Science Foundation of Shandong Province of China [ZR2014DQ014];
Technology Research and Development Program of Shandong Province of
China [2013GGF01022]; State Key Laboratory of Hydraulics and Mountain
River Engineering under Open Fund [SKHL1310]; Open Research Fund Program
of State Key Laboratory of Water Resources and Hydropower Engineering
Science [2011B079]
FX This work was supported in part by Natural Science Foundation of China
(No. 41361022 and 41171020) and Guangxi Science and Technology
Development Project (No. 2014DD29090), in part by Natural Science
Foundation of Shandong Province of China (ZR2014DQ014), Technology
Research and Development Program of Shandong Province of China
(2013GGF01022), and in part by the State Key Laboratory of Hydraulics
and Mountain River Engineering under Open Fund (SKHL1310) and Open
Research Fund Program of State Key Laboratory of Water Resources and
Hydropower Engineering Science (No. 2011B079). (Corresponding author:
Jianrong Cao.)
NR 26
TC 0
Z9 0
U1 8
U2 12
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 SEP
PY 2015
VL 8
IS 9
SI SI
BP 4568
EP 4580
DI 10.1109/JSTARS.2015.2483484
PG 13
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA CZ8AW
UT WOS:000367323300033
ER
PT J
AU Jin, YF
Goulden, ML
Faivre, N
Veraverbeke, S
Sun, FP
Hall, A
Hand, MS
Hook, S
Randerson, JT
AF Jin, Yufang
Goulden, Michael L.
Faivre, Nicolas
Veraverbeke, Sander
Sun, Fengpeng
Hall, Alex
Hand, Michael S.
Hook, Simon
Randerson, James T.
TI Identification of two distinct fire regimes in Southern California:
implications for economic impact and future change
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE fire regime; economic impact; fuel management; climate change; Santa Ana
winds
ID NORTHERN BAJA-CALIFORNIA; LAKE TAHOE BASIN; CLIMATE-CHANGE; WILDLAND
FIRES; UNITED-STATES; WILDFIRE; EXPENDITURES; TEMPERATURE; REANALYSIS;
SHIFTS
AB The area burned by Southern California wildfires has increased in recent decades, with implications for human health, infrastructure, and ecosystem management. Meteorology and fuel structure are universally recognized controllers of wildfire, but their relative importance, and hence the efficacy of abatement and suppression efforts, remains controversial. Southern California's wildfires can be partitioned by meteorology: fires typically occur either during Santa Ana winds (SA fires) in October through April, or warm and dry periods in June through September (non-SA fires). Previous work has not quantitatively distinguished between these fire regimes when assessing economic impacts or climate change influence. Here we separate five decades of fire perimeters into those coinciding with and without SA winds. The two fire types contributed almost equally to burned area, yet SA fires were responsible for 80% of cumulative 1990-2009 economic losses ($3.1 Billion). The damage disparity was driven by fire characteristics: SA fires spread three times faster, occurred closer to urban areas, and burned into areas with greater housing values. Non-SA fires were comparatively more sensitive to age-dependent fuels, often occurred in higher elevation forests, lasted for extended periods, and accounted for 70% of total suppression costs. An improved distinction of fire type has implications for future projections and management. The area burned in non-SA fires is projected to increase 77% (+/- 43%) by the mid-21st century with warmer and drier summers, and the SA area burned is projected to increase 64% (+/- 76%), underscoring the need to evaluate the allocation and effectiveness of suppression investments.
C1 [Jin, Yufang] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA.
[Jin, Yufang; Goulden, Michael L.; Faivre, Nicolas; Veraverbeke, Sander; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Sun, Fengpeng; Hall, Alex] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Hand, Michael S.] US Forest Serv, USDA, Rocky Mt Res Stn, Missoula, MT USA.
[Hook, Simon] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Jin, YF (reprint author), Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA.
EM yujin@ucdavis.edu
RI Hook, Simon/D-5920-2016; Hall, Alex/D-8175-2014; Veraverbeke,
Sander/H-2301-2012; Goulden, Michael/B-9934-2008;
OI Hook, Simon/0000-0002-0953-6165; Veraverbeke,
Sander/0000-0003-1362-5125; Goulden, Michael/0000-0002-9379-3948
FU NASA [NNX10AL14G]; Jenkins Family Foundation
FX This research was supported by NASA grant NNX10AL14G and the Jenkins
Family Foundation. We are also grateful to Dr H Safford for his comments
and Drs K Gebert and D Sapsis for their help with acquiring and
interpreting the economic data.
NR 44
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Z9 5
U1 12
U2 28
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD SEP
PY 2015
VL 10
IS 9
AR 094005
DI 10.1088/1748-9326/10/9/094005
PG 12
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CZ5KJ
UT WOS:000367141000008
ER
PT J
AU Mao, JF
Fu, WT
Shi, XY
Ricciuto, DM
Fisher, JB
Dickinson, RE
Wei, YX
Shem, W
Piao, SL
Wang, KC
Schwalm, CR
Tian, HQ
Mu, MQ
Arain, A
Ciais, P
Cook, R
Dai, YJ
Hayes, D
Hoffman, FM
Huang, MY
Huang, S
Huntzinger, DN
Ito, A
Jain, A
King, AW
Lei, HM
Lu, CQ
Michalak, AM
Parazoo, N
Peng, CH
Peng, SS
Poulter, B
Schaefer, K
Jafarov, E
Thornton, PE
Wang, WL
Zeng, N
Zeng, ZZ
Zhao, F
Zhu, QA
Zhu, ZC
AF Mao, Jiafu
Fu, Wenting
Shi, Xiaoying
Ricciuto, Daniel M.
Fisher, Joshua B.
Dickinson, Robert E.
Wei, Yaxing
Shem, Willis
Piao, Shilong
Wang, Kaicun
Schwalm, Christopher R.
Tian, Hanqin
Mu, Mingquan
Arain, Altaf
Ciais, Philippe
Cook, Robert
Dai, Yongjiu
Hayes, Daniel
Hoffman, Forrest M.
Huang, Maoyi
Huang, Suo
Huntzinger, Deborah N.
Ito, Akihiko
Jain, Atul
King, Anthony W.
Lei, Huimin
Lu, Chaoqun
Michalak, Anna M.
Parazoo, Nicholas
Peng, Changhui
Peng, Shushi
Poulter, Benjamin
Schaefer, Kevin
Jafarov, Elchin
Thornton, Peter E.
Wang, Weile
Zeng, Ning
Zeng, Zhenzhong
Zhao, Fang
Zhu, Qiuan
Zhu, Zaichun
TI Disentangling climatic and anthropogenic controls on global terrestrial
evapotranspiration trends
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE evapotranspiration; natural and anthropogenic controls; factorial
analysis; MsTMIP
ID MODEL INTERCOMPARISON PROJECT; PROGRAM MULTISCALE SYNTHESIS; WATER
CYCLE; CARBON-DIOXIDE; HYDROLOGICAL CYCLE; UNITED-STATES; TIME-SERIES;
RISING CO2; LAND-USE; VEGETATION
AB We examined natural and anthropogenic controls on terrestrial evapotranspiration (ET) changes from 1982 to 2010 using multiple estimates from remote sensing-based datasets and process-oriented land surface models. A significant increasing trend of ET in each hemisphere was consistently revealed by observationally-constrained data and multi-model ensembles that considered historic natural and anthropogenic drivers. The climate impacts were simulated to determine the spatiotemporal variations in ET. Globally, rising CO2 ranked second in these models after the predominant climatic influences, and yielded decreasing trends in canopy transpiration and ET, especially for tropical forests and high-latitude shrub land. Increasing nitrogen deposition slightly amplified global ET via enhanced plant growth. Land-use-induced ET responses, albeit with substantial uncertainties across the factorial analysis, were minor globally, but pronounced locally, particularly over regions with intensive land-cover changes. Our study highlights the importance of employing multi-stream ET and ET-component estimates to quantify the strengthening anthropogenic fingerprint in the global hydrologic cycle.
C1 [Mao, Jiafu; Shi, Xiaoying; Ricciuto, Daniel M.; Wei, Yaxing; Shem, Willis; Cook, Robert; Hayes, Daniel; King, Anthony W.; Thornton, Peter E.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA.
[Mao, Jiafu; Shi, Xiaoying; Ricciuto, Daniel M.; Wei, Yaxing; Shem, Willis; Cook, Robert; Hayes, Daniel; King, Anthony W.; Thornton, Peter E.] Oak Ridge Natl Lab, Climate Change Sci Inst, Oak Ridge, TN 37831 USA.
[Fu, Wenting; Dickinson, Robert E.] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA.
[Fisher, Joshua B.; Parazoo, Nicholas] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Piao, Shilong; Zeng, Zhenzhong] Peking Univ, Sino French Inst Earth Syst Sci, Coll Urban & Environm Sci, Beijing 100871, Peoples R China.
[Wang, Kaicun; Dai, Yongjiu] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China.
[Schwalm, Christopher R.] No Arizona Univ, Ctr Ecosyst Sci & Soc, Flagstaff, AZ 86011 USA.
[Schwalm, Christopher R.; Huntzinger, Deborah N.] No Arizona Univ, Sch Earth Sci & Environm Sustainabil, Flagstaff, AZ 86011 USA.
[Tian, Hanqin; Lu, Chaoqun] Auburn Univ, Int Ctr Climate & Global Change Res, Auburn, AL 36849 USA.
[Tian, Hanqin; Lu, Chaoqun] Auburn Univ, Sch Forestry & Wildlife Sci, Auburn, AL 36849 USA.
[Mu, Mingquan] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Arain, Altaf; Huang, Suo] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON, Canada.
[Arain, Altaf; Huang, Suo] McMaster Univ, McMaster Ctr Climate Change, Hamilton, ON, Canada.
[Ciais, Philippe; Peng, Shushi] LSCE, F-91191 Gif Sur Yvette, France.
[Hoffman, Forrest M.] Oak Ridge Natl Lab, Climate Change Sci Inst, Oak Ridge, TN 37831 USA.
[Hoffman, Forrest M.] Oak Ridge Natl Lab, Comp Sci & Math Div, Oak Ridge, TN 37831 USA.
[Huang, Maoyi] Pacific NW Natl Lab, Atmospher Sci & Global Change Div, Richland, WA 99354 USA.
[Huntzinger, Deborah N.] No Arizona Univ, Dept Civil Engn Construct Management & Environm E, Flagstaff, AZ 86011 USA.
[Ito, Akihiko] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan.
[Jain, Atul] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA.
[Lei, Huimin] Tsinghua Univ, Dept Hydraul Engn, Beijing 100084, Peoples R China.
[Michalak, Anna M.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[Peng, Changhui; Zhu, Qiuan] Univ Quebec Montreal, Inst Environm Sci, Montreal, PQ H3C 3P8, Canada.
[Poulter, Benjamin] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA.
[Schaefer, Kevin; Jafarov, Elchin] Univ Colorado, Natl Snow & Ice Data Ctr, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Zeng, Ning; Zhao, Fang] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Zeng, Ning; Zhao, Fang] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Zhu, Zaichun] Northwest A&F Univ, State Key Lab Soil Eros & Dryland Farming Loess P, Yangling 712100, Peoples R China.
RP Mao, JF (reprint author), Oak Ridge Natl Lab, Div Environm Sci, POB 2008, Oak Ridge, TN 37831 USA.
EM maoj@ornl.gov
RI Wang, Kaicun/F-7813-2012; Thornton, Peter/B-9145-2012; Jafarov,
Elchin/G-1616-2016; Lei, Huimin/H-9596-2015; Ricciuto,
Daniel/I-3659-2016; Zeng, Ning/A-3130-2008; Jain, Atul/D-2851-2016;
Hoffman, Forrest/B-8667-2012; Mao, Jiafu/B-9689-2012; Dai,
Yongjiu/D-6261-2014;
OI Cook, Robert/0000-0001-7393-7302; Fisher, Joshua/0000-0003-4734-9085;
Poulter, Benjamin/0000-0002-9493-8600; PENG, Shushi/0000-0001-5098-726X;
Huang, Maoyi/0000-0001-9154-9485; Wang, Kaicun/0000-0002-7414-5400;
Thornton, Peter/0000-0002-4759-5158; Jafarov,
Elchin/0000-0002-8310-3261; Lei, Huimin/0000-0002-1175-2334; Ricciuto,
Daniel/0000-0002-3668-3021; Zeng, Ning/0000-0002-7489-7629; Jain,
Atul/0000-0002-4051-3228; Hoffman, Forrest/0000-0001-5802-4134; Mao,
Jiafu/0000-0002-2050-7373; Dai, Yongjiu/0000-0002-3588-6644; Tian,
Hanqin/0000-0002-1806-4091
FU Terrestrial Ecosystem Science Scientific Focus Area (SFA) - Terrestrial
Ecosystem Science (TES) Program in the Climate and Environmental
Sciences Division (CESD) of the Biological and Environmental Research
Program; Biogeochemistry-Climate Feedbacks SFA - Regional and Global
Climate Modeling (RGCM) Program in the Climate and Environmental
Sciences Division (CESD) of the Biological and Environmental Research
Program in the US Department of Energy Office of Science; Regional and
Global Climate Modeling (RGCM) Program in the Climate and Environmental
Sciences Division (CESD) of the Biological and Environmental Research
Program in the US Department of Energy Office of Science [DE-SC0012534];
National Aeronautics and Space Administration (NASA) [NNX12AP74G,
NNX10AG01A, NNX11AO08A]; NASA; NASA ROSES [NNX10AG01A, NNH10AN681];
Natural Sciences and Engineering Research Council (NSERC) of Canada; US
Department of Energy (DOE), Office of Science, Biological and
Environmental Research; DOE [DE-AC05-00OR22725]; US Department of Energy
(DOE), Office of Science, Biological and Environmental Research (BER)
through Earth System Modeling program; U.S. DOE-BER; U.S. DOE-BER
through Subsurface Biogeochemical Research Program (SBR) as part of the
SBR Scientific Focus Area (SFA) at the Pacific Northwest National
Laboratory (PNNL); US DOE by BATTELLE Memorial Institute
[DE-AC05-76RLO1830]; NASA Interdisciplinary Science Program (IDS); NASA
Land Cover/Land Use Change Program (LCLUC); NASA Terrestrial Ecology
Program; NASA Atmospheric Composition Modeling and Analysis Program
(ACMAP); NSF Dynamics of Coupled Natural-Human System Program (CNH);
Decadal and Regional Climate Prediction using Earth System Models
(EaSM); DOE National Institute for Climate Change Research; USDA AFRI
Program; EPA STAR Program; US National Science Foundation
[NSF-AGS-12-43071, NSF-EFRI-083598]; USDA National Institute of Food and
Agriculture (NIFA) [2011-68002-30220]; US Department of Energy (DOE)
Office of Science [DOE-DE-SC0006706]; NASA Land cover and Land Use
Change Program [NNX14AD94G]; Office of Science of the US Department of
Energy [DE-AC02-05CH11231]; National Science Foundation [OCI-0725070,
ACI-1238993]; state of Illinois; GhG Europe FP7 grant; US Department of
Energy [DE-AC05-00OR22725]; DOE
FX This research was supported partially by the Terrestrial Ecosystem
Science Scientific Focus Area (SFA), which is sponsored by the
Terrestrial Ecosystem Science (TES) Program in the Climate and
Environmental Sciences Division (CESD) of the Biological and
Environmental Research Program in the US Department of Energy Office of
Science. This research was supported partially by the
Biogeochemistry-Climate Feedbacks SFA and project under contract of
DE-SC0012534, which are both sponsored by the Regional and Global
Climate Modeling (RGCM) Program in the Climate and Environmental
Sciences Division (CESD) of the Biological and Environmental Research
Program in the US Department of Energy Office of Science. CRS was
supported by National Aeronautics and Space Administration (NASA) Grants
#NNX12AP74G, #NNX10AG01A, and #NNX11AO08A. JBF carried out this research
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with NASA. Funding for the Multi-scale synthesis and
Terrestrial Model Intercomparison Project (MsTMIP,
http://nacp.ornl.gov/MsTMIP.shtml) activity was provided through NASA
ROSES Grant #NNX10AG01A. Data management support for preparing,
documenting, and distributing model driver and output data was performed
by the Modeling and Synthesis Thematic Data Center at Oak Ridge National
Laboratory (ORNL, http://nacp.ornl.gov), with funding through NASA ROSES
Grant #NNH10AN681. Finalized MsTMIP data products are archived at the
ORNL DAAC (http://daac.ornl.gov). This is MsTMIP contribution #5.;
CLASS-CTEM-N+: This research was funded by the Natural Sciences and
Engineering Research Council (NSERC) of Canada Discovery and Strategic
grants. CLASS and CTEM models were originally developed by the Climate
Research Branch and Canadian Centre for Climate Modelling and Analysis
(CCCMa) of Environment Canada, respectively.; CLM: This research is
supported in part by the US Department of Energy (DOE), Office of
Science, Biological and Environmental Research. Oak Ridge National
Laboratory is managed by UT-Battelle, LLC for DOE under contract
DE-AC05-00OR22725.; CLM4VIC: CLM4VIC simulations were supported in part
by the US Department of Energy (DOE), Office of Science, Biological and
Environmental Research (BER) through the Earth System Modeling program,
and performed using the Environmental Molecular Sciences Laboratory
(EMSL), a national scientific user facility sponsored by the U.S.
DOE-BER and located at Pacific Northwest National Laboratory (PNNL).
Participation of M Huang in the MsTMIP synthesis is supported by the
U.S. DOE-BER through the Subsurface Biogeochemical Research Program
(SBR) as part of the SBR Scientific Focus Area (SFA) at the Pacific
Northwest National Laboratory (PNNL). PNNL is operated for the US DOE by
BATTELLE Memorial Institute under contract DE-AC05-76RLO1830.; DLEM: The
Dynamic Land Ecosystem Model (DLEM) developed in the International
Center for Climate and Global Change Research at Auburn University has
been supported by NASA Interdisciplinary Science Program (IDS), NASA
Land Cover/Land Use Change Program (LCLUC), NASA Terrestrial Ecology
Program, NASA Atmospheric Composition Modeling and Analysis Program
(ACMAP); NSF Dynamics of Coupled Natural-Human System Program (CNH),
Decadal and Regional Climate Prediction using Earth System Models
(EaSM); DOE National Institute for Climate Change Research; USDA AFRI
Program and EPA STAR Program.; Integrated Science Assessment Model
(ISAM) simulations were supported by the US National Science Foundation
(NSF-AGS-12-43071 and NSF-EFRI-083598), the USDA National Institute of
Food and Agriculture (NIFA) (2011-68002-30220), the US Department of
Energy (DOE) Office of Science (DOE-DE-SC0006706) and the NASA Land
cover and Land Use Change Program (NNX14AD94G). ISAM simulations were
carried out at the National Energy Research Scientific Computing Center
(NERSC), which is supported by the Office of Science of the US
Department of Energy under contract DE-AC02-05CH11231, and at the Blue
Waters sustained-petascale computing, University of Illinois at
Urbana-Champaign, which is supported by the National Science Foundation
(awards OCI-0725070 and ACI-1238993) and the state of Illinois.;
ORCHIDEE-LSCE: ORCHIDEE is a global land surface model developed at the
IPSL institute in France. The simulations were performed with the
support of the GhG Europe FP7 grant with computing facilities provided
by LSCE (Laboratoire des Sciences du Climat et de l'Environnement) or
TGCC (Tres Grand Centre de Calcul).; This manuscript has been authored
by UT-Battelle, LLC under Contract No. DE-AC05-00OR22725 with the US
Department of Energy. The United States Government retains and the
publisher, by accepting the article for publication, acknowledges that
the United States Government retains a non-exclusive, paid-up,
irrevocable, world-wide license to publish or reproduce the published
form of this manuscript, or allow others to do so, for United States
Government purposes. The Department of Energy will provide public access
to these results of federally sponsored research in accordance with the
DOE Public Access Plan
(http://energy.gov/downloads/doe-publicaccess-plan).
NR 95
TC 11
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U1 19
U2 44
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD SEP
PY 2015
VL 10
IS 9
AR 094008
DI 10.1088/1748-9326/10/9/094008
PG 13
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CZ5KJ
UT WOS:000367141000011
ER
PT J
AU Neufeld, MJ
Charles, JB
AF Neufeld, Michael J.
Charles, John B.
TI Practicing for space underwater: inventing neutral buoyancy training,
1963-1968
SO ENDEAVOUR
LA English
DT Article
AB Neutral buoyancy's value was far from obvious when human spaceflight began in 1961. Starting in 1964, Environmental Research Associates, a tiny company in the suburbs of Baltimore, developed the key innovations in an obscure research project funded by NASA's Langley Research Center. The new Houston center dismissed it until a mid-1966 EVA crisis, after which it rapidly took over. In parallel, NASA Marshall Space Flight Center developed many of the same techniques, as did many large aerospace corporations, yet the long-run technological impact of corporate activity was near zero. Because ERA and Marshall's pioneering activities led to the two long-running NASA training centers at Houston and Huntsville, those two organizations deserve primary credit for the construction of the neutral buoyancy technological system.
C1 [Neufeld, Michael J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
[Charles, John B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
EM neufeldm@si.edu
NR 77
TC 0
Z9 0
U1 0
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0160-9327
EI 1873-1929
J9 ENDEAVOUR
JI Endeavour
PD SEP-DEC
PY 2015
VL 39
IS 3-4
BP 147
EP 159
DI 10.1016/j.endeavour.2015.05.006
PG 13
WC History & Philosophy Of Science; Multidisciplinary Sciences
SC History & Philosophy of Science; Science & Technology - Other Topics
GA CY1JB
UT WOS:000366161400003
PM 26186978
ER
PT J
AU Zaman, KBMQ
Fagan, AF
Bridges, JE
Brown, CA
AF Zaman, K. B. M. Q.
Fagan, A. F.
Bridges, J. E.
Brown, C. A.
TI An experimental investigation of resonant interaction of a rectangular
jet with a flat plate
SO JOURNAL OF FLUID MECHANICS
LA English
DT Article
DE acroacoustics; jet noise; flow structure interactions
ID NOISE; MECHANISM; DUCT
AB The interaction between an 8:1 aspect ratio rectangular jet and a flat plate, placed parallel to the jet, is addressed in this study. At high subsonic conditions and for certain relative locations of the plate, a resonance takes place with accompanying audible tones. Even when the tone is not audible the sound pressure level spectra are often marked by conspicuous peaks. The frequencies of these peaks, as functions of the plate's length, its location relative to the jet as well as jet Mach number, are studied in an effort to understand the How mechanism. It is demonstrated that the tones are not due to a simple feedback between the nozzle exit and the plate's trailing edge; the leading edge also comes into play in determining the frequency. With parametric Variation, it is found that there is an order in the most energetic spectral peaks; their frequencies cluster in distinct bands. The lowest frequency band is explained by an acoustic feedback involving diffraction at the plate's leading edge. Under the resonant condition, a periodic flapping motion of the jet column is seen when viewed in a direction parallel to the plate. Phase-averaged Mach number data on a cross -stream plane near the plate's trailing edge illustrate that the jet cross-section goes through large contortions within the period of the tone. Farther downstream a clear 'axis switching' takes place for the time-averaged cross-section of the jet that does not occur otherwise for a non-resonant condition.
C1 [Zaman, K. B. M. Q.] NASA Glenn Res Ctr, Prop Div, Inlets & Nozzles Branch, Cleveland, OH 44135 USA.
[Fagan, A. F.] NASA Glenn Res Ctr, Commun & Intelligent Syst Div, Opt & Photon Branch, Cleveland, OH 44135 USA.
[Bridges, J. E.; Brown, C. A.] NASA Glenn Res Ctr, Prop Div, Acoust Branch, Cleveland, OH 44135 USA.
RP Zaman, KBMQ (reprint author), NASA Glenn Res Ctr, Prop Div, Inlets & Nozzles Branch, Cleveland, OH 44135 USA.
EM khairul.b.zaman@nasa.gov
FU Commercial Supersonic Technology (CST) Project of NASA's Advanced Air
Vehicles Program; Advanced Air Transport Technology (AATT) Project of
NASA's Advanced Air Vehicles Program
FX Thanks are due to Ms M. Clem for help with schlieren flow visualization
and to Drs S. Leib and B. Henderson for helpful inputs. Support from the
Commercial Supersonic Technology (CST) and Advanced Air Transport
Technology (AATT) Projects of NASA's Advanced Air Vehicles Program is
gratefully acknowledged.
NR 34
TC 0
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U1 1
U2 1
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 SEP
PY 2015
VL 779
BP 751
EP 775
DI 10.1017/jfm.2015.453
PG 25
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA CY4RU
UT WOS:000366396700008
ER
PT J
AU Knepp, T
Pippin, M
Crawford, J
Chen, G
Szykman, J
Long, R
Cowen, L
Cede, A
Abuhassan, N
Herman, J
Delgado, R
Compton, J
Berkoff, T
Fishman, J
Martins, D
Stauffer, R
Thompson, AM
Weinheimer, A
Knapp, D
Montzka, D
Lenschow, D
Neil, D
AF Knepp, T.
Pippin, M.
Crawford, J.
Chen, G.
Szykman, J.
Long, R.
Cowen, L.
Cede, A.
Abuhassan, N.
Herman, J.
Delgado, R.
Compton, J.
Berkoff, T.
Fishman, J.
Martins, D.
Stauffer, R.
Thompson, A. M.
Weinheimer, A.
Knapp, D.
Montzka, D.
Lenschow, D.
Neil, D.
TI Estimating surface NO2 and SO2 mixing ratios from fast-response total
column observations and potential application to geostationary missions
SO JOURNAL OF ATMOSPHERIC CHEMISTRY
LA English
DT Article
DE Nitrogen dioxide; Sulfur dioxide; Air quality; Remote sensing;
DISCOVER-AQ; CAPABLE; GEO-CAPE
ID TROPOSPHERIC NITROGEN-DIOXIDE; AIR-POLLUTION; MAX-DOAS; PARTICULATE
MATTER; URBAN-ENVIRONMENT; OZONE; ATMOSPHERE; INSTRUMENTS; SCIAMACHY;
SATELLITE
AB Total-column nitrogen dioxide (NO2) data collected by a ground-based sun-tracking spectrometer system (Pandora) and an photolytic-converter-based in-situ instrument collocated at NASA's Langley Research Center in Hampton, Virginia were analyzed to study the relationship between total-column and surface NO2 measurements. The measurements span more than a year and cover all seasons. Surface mixing ratios are estimated via application of a planetary boundary-layer (PBL) height correction factor. This PBL correction factor effectively corrects for boundary-layer variability throughout the day, and accounts for up to a parts per thousand 75 % of the variability between the NO2 data sets. Previous studies have made monthly and seasonal comparisons of column/surface data, which has shown generally good agreement over these long average times. In the current analysis comparisons of column densities averaged over 90 s and 1 h are made. Applicability of this technique to sulfur dioxide (SO2) is briefly explored. The SO2 correlation is improved by excluding conditions where surface levels are considered background. The analysis is extended to data from the July 2011 DISCOVER-AQ mission over the greater Baltimore, MD area to examine the method's performance in more-polluted urban conditions where NO2 concentrations are typically much higher.
C1 [Knepp, T.] Sci Syst & Applicat Inc, Hampton, VA 23681 USA.
[Knepp, T.; Pippin, M.; Crawford, J.; Chen, G.; Cowen, L.; Neil, D.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Szykman, J.; Long, R.] US EPA, Durham, NC 27701 USA.
[Cede, A.] LuftBlick, A-6162 Kreith, Austria.
[Cede, A.; Abuhassan, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Abuhassan, N.] Morgan State Univ, Sch Engn, Baltimore, MD 21251 USA.
[Herman, J.; Delgado, R.; Compton, J.; Berkoff, T.] Univ Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
[Fishman, J.] St Louis Univ, Dept Earth & Atmospher Sci, St Louis, MO 63103 USA.
[Martins, D.; Stauffer, R.; Thompson, A. M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Weinheimer, A.; Knapp, D.; Montzka, D.; Lenschow, D.] Natl Ctr Atmospher Res, Boulder, CO 80305 USA.
RP Knepp, T (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23681 USA.
EM travis.n.knepp@nasa.gov
RI Delgado, Ruben/F-9753-2016;
OI Delgado, Ruben/0000-0002-7133-2462; Herman, Jay/0000-0002-9146-1632;
Stauffer, Ryan/0000-0002-8583-7795; LENSCHOW, DONALD/0000-0003-4353-0098
FU NASA Applied Sciences Program; EPA collaborations under an EPA-LaRC
memorandum of agreement; GEO-CAPE mission studies; Langley Innovative
Partnership Program; NASA's post-doctoral program; National Science
Foundation
FX Funding for this work was provided by NASA Applied Sciences Program, EPA
collaborations under an EPA-LaRC memorandum of agreement, GEO-CAPE
mission studies, and Langley Innovative Partnership Program. T. Knepp
was supported through NASA's post-doctoral program. The National Center
for Atmospheric Research is sponsored by the National Science
Foundation. Although this paper has been reviewed by the EPA and
approved for publication, it does not necessarily reflect EPA policies
or views.
NR 56
TC 7
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U1 5
U2 18
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-7764
EI 1573-0662
J9 J ATMOS CHEM
JI J. Atmos. Chem.
PD SEP
PY 2015
VL 72
IS 3-4
SI SI
BP 261
EP 286
DI 10.1007/s10874-013-9257-6
PG 26
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CX6CP
UT WOS:000365789100005
ER
PT J
AU Tzortziou, M
Herman, JR
Cede, A
Loughner, CP
Abuhassan, N
Naik, S
AF Tzortziou, Maria
Herman, Jay R.
Cede, Alexander
Loughner, Christopher P.
Abuhassan, Nader
Naik, Sheenali
TI Spatial and temporal variability of ozone and nitrogen dioxide over a
major urban estuarine ecosystem
SO JOURNAL OF ATMOSPHERIC CHEMISTRY
LA English
DT Article
DE Ozone; Nitrogen dioxide; Atmospheric variability; Urban; Coastal; Remote
sensing
ID ATMOSPHERIC CORRECTION; MONITORING INSTRUMENT; NO2 ABSORPTION;
ALGORITHMS; IRRADIANCE; RETRIEVAL; TRANSPORT; DEPLETION; QUALITY; SYSTEM
AB Spatial and temporal dynamics in trace gas pollutants were examined over a major urban estuarine ecosystem, using a new network of ground-based Pandora spectrometers deployed at strategic locations along the Washington-Baltimore corridor and the Chesapeake Bay. Total column ozone (TCO3) and nitrogen dioxide (TCNO2) were measured during NASA's DISCOVER-AQ and GeoCAPE-CBODAQ campaigns in July 2011. The Pandora network provided high-resolution information on air-quality variability, local pollution conditions, large-scale meteorological influences, and interdependencies of ozone and its major precursor, NO2. Measurements were used to compare with air-quality model simulations (CMAQ), evaluate Aura-OMI satellite retrievals, and assess advantages and limitations of space-based observations under a range of conditions. During the campaign, TCNO2 varied by an order of magnitude, both spatially and temporally. Although fairly constant in rural regions, TCNO2 showed clear diurnal and weekly patterns in polluted urban areas caused by changes in near-surface emissions. With a coarse resolution and an overpass at around 13:30 local time, OMI cannot detect this strong variability in NO2, missing pollution peaks from industrial and rush hour activities. Not as highly variable as NO2, TCO3 was mostly affected by large-scale meteorological patterns as observed by OMI. A clear weekly cycle in TCO3, with minima over the weekend, was due to a combination of weekly weather patterns and changes in near-surface NOx emissions. A Pandora instrument intercomparison under the same conditions at GSFC showed excellent agreement, within +/- 4.8DU for TCO3 and +/- 0.07DU for TCNO2 with no air-mass-factor dependence, suggesting that observed variability during the campaign was real.
C1 [Tzortziou, Maria; Loughner, Christopher P.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Tzortziou, Maria; Herman, Jay R.; Cede, Alexander; Loughner, Christopher P.; Abuhassan, Nader] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Herman, Jay R.; Abuhassan, Nader] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Cede, Alexander] LuftBlick, Kreith, Austria.
[Naik, Sheenali] Univ Maryland, Environm Sci & Policy Dept, College Pk, MD 20742 USA.
RP Tzortziou, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM maria.a.tzortziou@nasa.gov
OI Herman, Jay/0000-0002-9146-1632; Loughner,
Christopher/0000-0002-3833-2014
FU National Aeronautics and Space Administration (NASA) DISCOVER-AQ project
[NNX10AR39G]; NASA CBODAQ field campaign; [NASA.NNX10AQ79G];
[NASA.NNX11AP07G]
FX This work was supported under the National Aeronautics and Space
Administration (NASA) DISCOVER-AQ project (Grant: NNX10AR39G) and the
NASA CBODAQ field campaign, with additional support from grants
NASA.NNX10AQ79G and NASA.NNX11AP07G. The authors would like to thank
Christian Retscher, James H. Crawford, Kenneth E. Pickering, Antonio
Mannino, and two anonymous reviewers for their constructive comments and
suggestions for improvement of the manuscript.
NR 59
TC 7
Z9 7
U1 3
U2 19
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-7764
EI 1573-0662
J9 J ATMOS CHEM
JI J. Atmos. Chem.
PD SEP
PY 2015
VL 72
IS 3-4
SI SI
BP 287
EP 309
DI 10.1007/s10874-013-9255-8
PG 23
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CX6CP
UT WOS:000365789100006
ER
PT J
AU Thompson, AM
Stauffer, RM
Miller, SK
Martins, DK
Joseph, E
Weinheimer, AJ
Diskin, GS
AF Thompson, Anne M.
Stauffer, Ryan M.
Miller, Sonya K.
Martins, Douglas K.
Joseph, Everette
Weinheimer, Andrew J.
Diskin, Glenn S.
TI Ozone profiles in the Baltimore-Washington region (2006-2011): satellite
comparisons and DISCOVER-AQ observations
SO JOURNAL OF ATMOSPHERIC CHEMISTRY
LA English
DT Article
DE Tropospheric ozone; Stratosphere-troposphere exchange; Satellite
validation; DISCOVER-AQ; Baltimore pollution; Ozonesondes; Washington DC
pollution; Air quality; Carbon monoxide; Aircraft chemical measurements
ID AIR-MASS CHARACTERISTICS; TROPOSPHERIC OZONE; UNITED-STATES; ATLANTIC;
POLLUTION; PACIFIC
AB Much progress has been made in creating satellite products for tracking the pollutants ozone and NO2 in the troposphere. Yet, in mid-latitude regions where meteorological interactions with pollutants are complex, accuracy can be difficult to achieve, largely due to persistent layering of some constituents. We characterize the layering of ozone soundings and related species measured from aircraft over two ground sites in suburban Washington, DC (Beltsville, MD, 39.05 N; 76.9 W) and Baltimore (Edgewood, MD, 39.4 N; 76.3 W) during the July 2011 DISCOVER-AQ (Deriving Information on Surface Conditions from Column and Vertically Resolved Observations Relevant to Air Quality) experiment. First, we compare column-ozone amounts from the Beltsville and Edgewood sondes with data from overpassing satellites. Second, processes influencing ozone profile structure are analyzed using Laminar Identification and tracers: sonde water vapor, aircraft CO and NOy. Third, Beltsville ozone profiles and meteorological influences in July 2011 are compared to those from the summers of 2006-2010. Sonde-satellite offsets in total ozone during July 2011 at Edgewood and Beltsville, compared to the Ozone Monitoring Instrument (OMI), were 3 % mean absolute error, not statistically significant. The disagreement between an OMI/Microwave Limb Sounder-based tropospheric ozone column and the sonde averaged 10 % at both sites, with the sonde usually greater than the satellite. Laminar Identification (LID), that distinguishes ozone segments influenced by convective and advective transport, reveals that on days when both stations launched ozonesondes, vertical mixing was stronger at Edgewood. Approximately half the lower free troposphere sonde profiles have very dry laminae, with coincident aircraft spirals displaying low CO (80-110 ppbv), suggesting stratospheric influence. Ozone budgets at Beltsville in July 2011, determined with LID, as well as standard meteorological indicators, resemble those of 4 of the previous 5 summers. The penetration of stratospheric air throughout the troposphere appears to be typical for summer conditions in the Baltimore-Washington region.
C1 [Thompson, Anne M.; Stauffer, Ryan M.; Miller, Sonya K.; Martins, Douglas K.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Joseph, Everette] Howard Univ, Dept Phys & Astron, Washington, DC 20059 USA.
[Weinheimer, Andrew J.] NCAR, Div Atmospher Chem, Boulder, CO 80307 USA.
[Diskin, Glenn S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Thompson, AM (reprint author), NASA, Goddard Space Flight Ctr, Code 614, Greenbelt, MD 20771 USA.
EM anne.m.thompson@nasa.gov; rms5539@psu.edu; Sck117@psu.edu;
Dkm18@psu.edu; ejoseph@howard.edu; wein@ucar.edu;
glenn.s.diskin@nasa.gov
RI Thompson, Anne /C-3649-2014;
OI Thompson, Anne /0000-0002-7829-0920; Stauffer, Ryan/0000-0002-8583-7795
FU NASA [NNG10AJ38]; NASA's Tropospheric Chemistry Program [NNG06GB18G,
NNX08AJ15G]; Howard University BCCSO [NNX10Q11A]; AQAST (Air Quality
Applied Sciences Team) [NNX11AQ44G]
FX We are grateful to the DISCOVER-AQ leadership (J. H. Crawford, PI; K. E.
Pickering, Project Scientist; M. M. Kleb, Deputy) for overall design,
planning and execution of the Maryland phase of the project. A number of
people provided additional support and scientific insights for
Beltsville (R. Sakai, M. Payne, J. Fuentes) and the NATIVE site at
Edgewood (H. Halliday, N. Abuhassan, J. Herman, T. Berkoff, R. Delgado,
P. Decola, D. M. Giles, the Leosphere group). R. R. Dickerson (Univ.
Maryland), W. F. Ryan (PSU) and the folks at MDE provided invaluable
perspective on pollution in the Baltimore-Edgewood area. Penn State's
participation in DISCOVER-AQ is sponsored by NASA Grant NNG10AJ38.
Additional support for data collection and analysis was provided by
NASA's Tropospheric Chemistry Program (Grants NNG06GB18G and
NNX08AJ15G), Howard University BCCSO (NNX10Q11A) and AQAST (Air Quality
Applied Sciences Team, Grant NNX11AQ44G). J. A Bielli and J. M. Festa
(PSU) carried out some of the early analyses.
NR 38
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U1 6
U2 17
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-7764
EI 1573-0662
J9 J ATMOS CHEM
JI J. Atmos. Chem.
PD SEP
PY 2015
VL 72
IS 3-4
SI SI
BP 393
EP 422
DI 10.1007/s10874-014-9283-z
PG 30
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CX6CP
UT WOS:000365789100011
ER
PT J
AU O'Halloran, TL
Fuentes, JD
Tao, WK
Li, X
AF O'Halloran, T. L.
Fuentes, J. D.
Tao, W. K.
Li, X.
TI Sensitivity of convection to observed variation in aerosol size
distributions and composition at a rural site in the southeastern United
States
SO JOURNAL OF ATMOSPHERIC CHEMISTRY
LA English
DT Article
DE Aerosol indirect effect; Biogenic aerosols; Cloud condensation nuclei
(CCN); Convection; Precipitation enhancement; New particle formation
ID CLOUD CONDENSATION NUCLEI; SYSTEM-RESOLVING MODEL; PART I; ATMOSPHERIC
AEROSOLS; ORGANIC AEROSOLS; MICROPHYSICS; PRECIPITATION; CUMULUS;
SIMULATIONS; PARTICLES
AB We present a sensitivity analysis to determine the impact of variations in aerosol physical and chemical characteristics, as observed in the field in the southeastern United States, on convective cloud microphysics. Scenarios reflecting changes in aerosol properties, observed over the Piedmont of Virginia and associated with new particle formation and growth events, were evaluated using the two-dimensional version of the Goddard Cumulus Ensemble Model with detailed spectral-bin microphysics. Two aerosol size distributions represented early and late stages of particle growth, and two aerosol chemical compositions (norpinic acid and ammonium sulfate) represented extremes in aerosol hygroscopicity observed at the field site, for a total of four scenarios. The chosen compositions reflect inferred local changes in aerosol composition over short time scales. Variations in the aerosol size distribution and composition resulted in substantial variation in the total number of cloud condensation nuclei (CCN) produced in the four case studies. Cases with high CCN concentrations developed larger, more vigorous clouds with more precipitation generated by both warm and cold rain processes. Greater numbers of drops were propelled aloft and formed an extensive ice anvil that produced a large area of stratiform rain. Convection was enhanced by increasing aerosols despite decreases in precipitation efficiency. In contrast, lower CCN concentrations developed smaller clouds with suppressed cold rain processes and less total precipitation. The relatively small increase in CCN concentration associated with the increase in aerosol hygroscopicity resulted in an increase in accumulated modeled precipitation of 12 % after 180 min of simulation time in both high and low CCN cases. The increase in accumulated precipitation due to the substantial increase in CCN concentration associated with growth of the aerosol size distribution was 93 % for both aerosol compositions. The timing of the onset of precipitation was not affected by aerosol concentration or composition.
C1 [O'Halloran, T. L.] Sweet Briar Coll, Dept Environm Sci, Sweet Briar, VA 24595 USA.
[Fuentes, J. D.] Penn State Univ, Dept Meteorol, State Coll, PA 16802 USA.
[Tao, W. K.; Li, X.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Branch, Greenbelt, MD 20771 USA.
[Li, X.] Morgan State Univ, GESTAR Program, Baltimore, MD 21251 USA.
RP O'Halloran, TL (reprint author), Sweet Briar Coll, Dept Environm Sci, Sweet Briar, VA 24595 USA.
EM tohalloran@sbc.edu
RI Measurement, Global/C-4698-2015
FU NASA [NAG5-13778]
FX NASA provided funding in support of this research (grant number
NAG5-13778).
NR 61
TC 1
Z9 1
U1 3
U2 9
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-7764
EI 1573-0662
J9 J ATMOS CHEM
JI J. Atmos. Chem.
PD SEP
PY 2015
VL 72
IS 3-4
SI SI
BP 441
EP 454
DI 10.1007/s10874-015-9300-x
PG 14
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CX6CP
UT WOS:000365789100013
ER
PT J
AU Reed, AJ
Thompson, AM
Kollonige, DE
Martins, DK
Tzortziou, MA
Herman, JR
Berkoff, TA
Abuhassan, NK
Cede, A
AF Reed, Andra J.
Thompson, Anne M.
Kollonige, Debra E.
Martins, Douglas K.
Tzortziou, Maria A.
Herman, Jay R.
Berkoff, Timothy A.
Abuhassan, Nader K.
Cede, Alexander
TI Effects of local meteorology and aerosols on ozone and nitrogen dioxide
retrievals from OMI and pandora spectrometers in Maryland, USA during
DISCOVER-AQ 2011
SO JOURNAL OF ATMOSPHERIC CHEMISTRY
LA English
DT Article
DE Ozone Monitoring Instrument (OMI); Pandora; Total column ozone; Total
column nitrogen dioxide; Atmospheric chemistry; DISCOVER-AQ
ID CLIMATOLOGY; INSTRUMENT; ALGORITHM; PRODUCTS; TOMS
AB An analysis is presented for both ground- and satellite-based retrievals of total column ozone and nitrogen dioxide levels from the Washington, D.C., and Baltimore, Maryland, metropolitan area during the NASA-sponsored July 2011 campaign of Deriving Information on Surface COnditions from Column and VERtically Resolved Observations Relevant to Air Quality (DISCOVER-AQ). Satellite retrievals of total column ozone and nitrogen dioxide from the Ozone Monitoring Instrument (OMI) on the Aura satellite are used, while Pandora spectrometers provide total column ozone and nitrogen dioxide amounts from the ground. We found that OMI and Pandora agree well (residuals within +/- 25 % for nitrogen dioxide, and +/- 4.5 % for ozone) for a majority of coincident observations during July 2011. Comparisons with surface nitrogen dioxide from a Teledyne API 200 EU NOx Analyzer showed nitrogen dioxide diurnal variability that was consistent with measurements by Pandora. However, the wide OMI field of view, clouds, and aerosols affected retrievals on certain days, resulting in differences between Pandora and OMI of up to +/- 65 % for total column nitrogen dioxide, and +/- 23 % for total column ozone. As expected, significant cloud cover (cloud fraction > 0.2) was the most important parameter affecting comparisons of ozone retrievals; however, small, passing cumulus clouds that do not coincide with a high (> 0.2) cloud fraction, or low aerosol layers which cause significant backscatter near the ground affected the comparisons of total column nitrogen dioxide retrievals. Our results will impact post-processing satellite retrieval algorithms and quality control procedures.
C1 [Reed, Andra J.; Thompson, Anne M.; Kollonige, Debra E.; Martins, Douglas K.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Tzortziou, Maria A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Tzortziou, Maria A.; Herman, Jay R.; Abuhassan, Nader K.; Cede, Alexander] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Herman, Jay R.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA.
[Berkoff, Timothy A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA.
[Abuhassan, Nader K.] LuftBlick, Kreith, Austria.
[Cede, Alexander] Morgan State Univ, Sch Engn, Baltimore, MD 21239 USA.
RP Reed, AJ (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA.
EM axr5145@psu.edu
RI Thompson, Anne /C-3649-2014;
OI Thompson, Anne /0000-0002-7829-0920; Herman, Jay/0000-0002-9146-1632
FU National Aeronautics and Space Administration (NASA) DISCOVER-AQ grant
[NNX10AR39G]; [NNX08AJ15G]; [NNX10AQ11A]
FX This work was supported by a National Aeronautics and Space
Administration (NASA) DISCOVER-AQ grant (NNX10AR39G), with additional
support from NNX08AJ15G and NNX10AQ11A. The authors would like to thank
the co-PIs of DISCOVER-AQ James Crawford (NASA-LARC) and Kenneth
Pickering (NASA-GSFC), as well as the members of the Gator Research team
(PSU) for their support and contributions.
NR 37
TC 6
Z9 6
U1 1
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-7764
EI 1573-0662
J9 J ATMOS CHEM
JI J. Atmos. Chem.
PD SEP
PY 2015
VL 72
IS 3-4
SI SI
BP 455
EP 482
DI 10.1007/s10874-013-9254-9
PG 28
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CX6CP
UT WOS:000365789100014
ER
PT J
AU Ackermann, M
Ajello, M
Albert, A
Baldini, L
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Bissaldi, E
Bloom, ED
Bonino, R
Bregeon, J
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caragiulo, M
Caraveo, PA
Cecchi, C
Charles, E
Chekhtman, A
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cuoco, A
Cutini, S
D'Ammando, F
de Angelis, A
de Palma, F
Dermer, CD
Digel, SW
Drell, PS
Drlica-Wagner, A
Favuzzi, C
Ferrara, EC
Franckowiak, A
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Giordano, F
Giroletti, M
Godfrey, G
Guiriec, S
Gustafsson, M
Hewitt, JW
Hou, X
Kamae, T
Kuss, M
Larsson, S
Latronico, L
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Malyshev, D
Massaro, F
Mayer, M
Mazziotta, MN
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Negro, M
Nemmen, R
Nuss, E
Ohsugi, T
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Sanchez-Conde, M
Schulz, A
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Strong, AW
Suson, DJ
Tajima, H
Takahashi, H
Thayer, JG
Thayer, JB
Tibaldo, L
Tinivella, M
Torres, DF
Troja, E
Uchiyama, Y
Vianello, G
Werner, M
Winer, BL
Wood, KS
Wood, M
Zaharijas, G
AF Ackermann, M.
Ajello, M.
Albert, A.
Baldini, L.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Bissaldi, E.
Bloom, E. D.
Bonino, R.
Bregeon, J.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Caraveo, P. A.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cuoco, A.
Cutini, S.
D'Ammando, F.
de Angelis, A.
de Palma, F.
Dermer, C. D.
Digel, S. W.
Drell, P. S.
Drlica-Wagner, A.
Favuzzi, C.
Ferrara, E. C.
Franckowiak, A.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Giordano, F.
Giroletti, M.
Godfrey, G.
Guiriec, S.
Gustafsson, M.
Hewitt, J. W.
Hou, X.
Kamae, T.
Kuss, M.
Larsson, S.
Latronico, L.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Malyshev, D.
Massaro, F.
Mayer, M.
Mazziotta, M. N.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Negro, M.
Nemmen, R.
Nuss, E.
Ohsugi, T.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Sanchez-Conde, M.
Schulz, A.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Strong, A. W.
Suson, D. J.
Tajima, H.
Takahashi, H.
Thayer, J. G.
Thayer, J. B.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Troja, E.
Uchiyama, Y.
Vianello, G.
Werner, M.
Winer, B. L.
Wood, K. S.
Wood, M.
Zaharijas, G.
CA Fermi LAT Collaboration
TI Limits on dark matter annihilation signals from the Fermi LAT 4-year
measurement of the isotropic gamma-ray background
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE gamma ray experiments; dark matter theory; dark matter experiments; dark
matter simulations
ID LARGE-AREA TELESCOPE; RADIO GALAXIES; GALACTIC HALO; COSMOLOGICAL
PARAMETERS; MASS; RADIATION; EMISSION; MILKY; 1ST; ANISOTROPIES
AB We search for evidence of dark matter (DM) annihilation in the isotropic gamma-ray background (IGRB) measured with 50 months of Fermi Large Area Telescope (LAT) observations. An improved theoretical description of the cosmological DM annihilation signal, based on two complementary techniques and assuming generic weakly interacting massive particle (WIMP) properties, renders more precise predictions compared to previous work. More specifically, we estimate the cosmologically-induced gamma-ray intensity to have an uncertainty of a factor similar to 20 in canonical setups. We consistently include both the Galactic and extragalactic signals under the same theoretical framework, and study the impact of the former on the IGRB spectrum derivation. We find no evidence for a DM signal and we set limits on the DM-induced isotropic gamma-ray signal. Our limits are competitive for DM particle masses up to tens of TeV and, indeed, are the strongest limits derived from Fermi LAT data at TeV energies. This is possible thanks to the new Fermi LAT IGRB measurement, which now extends up to an energy of 820 GeV. We quantify uncertainties in detail and show the potential this type of search offers for testing the WIMP paradigm with a complementary and truly cosmological probe of DM particle signals.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Albert, A.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Franckowiak, A.; Funk, S.; Godfrey, G.; Kamae, T.; Malyshev, D.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Negro, M.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Tajima, H.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Albert, A.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Franckowiak, A.; Funk, S.; Godfrey, G.; Kamae, T.; Malyshev, D.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Negro, M.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Tajima, H.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Bissaldi, E.; Longo, F.; Zaharijas, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Chiaro, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bechtol, K.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Bissaldi, E.; Zaharijas, G.] Univ Trieste, I-34127 Trieste, Italy.
[Bonino, R.; Cuoco, A.; Latronico, L.; Negro, M.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bonino, R.; Cuoco, A.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France.
[Bruel, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caragiulo, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cecchi, C.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00133 Rome, Italy.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Roma, Italy.
[Conrad, J.; Larsson, S.; Sanchez-Conde, M.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.; Cuoco, A.; Larsson, S.; Sanchez-Conde, M.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy.
[de Palma, F.] Univ Grave Telemat Pegaso, I-80132 Naples, Italy.
[Dermer, C. D.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Drlica-Wagner, A.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Ferrara, E. C.; Guiriec, S.; Hewitt, J. W.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fukazawa, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Gustafsson, M.] Univ Libre Bruxelles, Serv Phys Theor, B-1050 Brussels, Belgium.
[Hewitt, J. W.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Hewitt, J. W.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Hewitt, J. W.] CRESST, Greenbelt, MD 20771 USA.
[Hou, X.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Massaro, F.] Yale Univ, Dept Phys, Dept Astron, New Haven, CT 06520 USA.
[Massaro, F.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Mitthumsiri, W.] Mahidol Univ, Dept Phys, Fac Sci, Bangkok 10400, Thailand.
[Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Murgia, S.] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA.
[Nemmen, R.] Univ Sao Paulo, Inst Astron Geofis & Cincias Atmosfer, BR-05508090 Sao Paulo, SP, Brazil.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Torres, D. F.] IEEC CSIC, Inst Space Sci, E-08193 Barcelona, Spain.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Zaharijas, G.] Abdus Salam Int Ctr Theoret Phys, I-34151 Trieste, Italy.
[Zaharijas, G.] Univ Nova Gorica, Lab Astroparticle Phys, SI-5000 Nova Gorica, Slovenia.
[Gustafsson, M.] Inst Theoret Phys, D-37077 Gottingen, Germany.
RP Franckowiak, A (reprint author), Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
EM afrancko@slac.stanford.edu;
michael.gustafsson@theorie.physik.uni-goettingen.de;
sanchezconde@fysik.su.se; gabrijela.zaharijas@ung.si
RI Morselli, Aldo/G-6769-2011; Reimer, Olaf/A-3117-2013; giglietto,
nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro,
Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016; Massaro,
Francesco/L-9102-2016; Torres, Diego/O-9422-2016; Orlando,
E/R-5594-2016; Funk, Stefan/B-7629-2015; Bonino, Raffaella/S-2367-2016;
OI Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385;
giglietto, nicola/0000-0002-9021-2888; Moskalenko,
Igor/0000-0001-6141-458X; Bissaldi, Elisabetta/0000-0001-9935-8106;
Massaro, Francesco/0000-0002-1704-9850; Torres,
Diego/0000-0002-1522-9065; Funk, Stefan/0000-0002-2012-0080; Sgro',
Carmelo/0000-0001-5676-6214; Zaharijas, Gabrijela/0000-0001-8484-7791;
SPINELLI, Paolo/0000-0001-6688-8864; orienti,
monica/0000-0003-4470-7094; Gargano, Fabio/0000-0002-5055-6395; Baldini,
Luca/0000-0002-9785-7726
FU Belgian Science Policy [TAP VII/37]; IISN; ARC project; Wenner-Gren
foundation; NASA [NNH09ZDA001N]
FX M.G. is supported by the Belgian Science Policy (TAP VII/37), the IISN
and the ARC project. M.A.S.C. acknowledges the support of the
Wenner-Gren foundation to develop his research and the NASA grant
NNH09ZDA001N for the study of the extragalactic background. G.Z. is
grateful to SLAC for hospitality during part of the realization of this
work. The authors are thankful to Emiliano Sefusatti for help with
producing some of the figures. We also thank Mattia Fornasa for useful
discussions and comments.
NR 123
TC 18
Z9 18
U1 1
U2 8
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 SEP
PY 2015
IS 9
AR 008
DI 10.1088/1475-7516/2015/09/008
PG 40
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CX4SG
UT WOS:000365690000008
ER
PT J
AU McElroy, MW
Lawrie, A
Bond, IP
AF McElroy, M. W.
Lawrie, A.
Bond, I. P.
TI Optimisation of an air film cooled CFRP panel with an embedded vascular
network
SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER
LA English
DT Article
DE Carbon fibre reinforced polymer; Film cooling; Microvascular; Thermal
analysis
AB The increasing use in the aerospace industry of strong, lightweight composite materials in primary structural components promises to substantially reduce aircraft non-pay-load weight, improving fuel consumption and operating profitability. This study explores the extension of composite material to regions of gas turbine engines previously considered too hot for composites with moderate melting points. Throughout the majority of a gas turbine cycle, gas stream temperatures exceed the polymer composite glass transition by a considerable margin. Boundary layer cooling strategies, however, may be adopted in the compression stages to extend the downstream distance that can be constructed using lightweight composites. This paper presents formulation and validation of a numerical model and its use in an optimisation study to develop a systematic process for thermal design of polymer composite structures in 'warm' gas streams. Internal vascular and external boundary layer film cooling strategies are considered. Published by Elsevier Ltd.
C1 [McElroy, M. W.] NASA, Durabil Damage Tolerance & Reliabil Branch, Langley Res Ctr, Hampton, VA USA.
[Lawrie, A.] Univ Bristol, Dept Mech Engn, Bristol, Avon, England.
[Bond, I. P.] Univ Bristol, Dept Aerosp Engn, Bristol, Avon, England.
RP McElroy, MW (reprint author), 2 W Reid St,Mail Stop 188E, Hampton, VA 23681 USA.
EM mark.w.mcelroy@nasa.gov
OI Bond, Ian/0000-0003-0526-5836
FU University of Bristol
FX This work was funded by The University of Bristol. The authors thank Dr.
Shahrokh Shahpar (Rolls Royce 3D Geometry, Meshing, and Optimisation,
Rolls Royce plc., Derby, UK) and Rolls-Royce for allowing us the use of
their proprietary optimisation software package, SOFT [24].
NR 23
TC 2
Z9 2
U1 1
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0017-9310
EI 1879-2189
J9 INT J HEAT MASS TRAN
JI Int. J. Heat Mass Transf.
PD SEP
PY 2015
VL 88
BP 284
EP 296
DI 10.1016/j.ijheatmasstransfer.2015.04.071
PG 13
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA CW2DZ
UT WOS:000364802600028
ER
PT J
AU Hartwig, J
Hu, H
Styborski, J
Chung, JN
AF Hartwig, Jason
Hu, Hong
Styborski, Jeremy
Chung, J. N.
TI Comparison of cryogenic flow boiling in liquid nitrogen and liquid
hydrogen chilldown experiments
SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER
LA English
DT Article
DE Nucleate boiling; Transition boiling; Chilldown; Liquid nitrogen; Liquid
hydrogen; Cryogenic heat transfer coefficient
ID CRITICAL HEAT-FLUX; TRANSFER COEFFICIENT; UNIVERSAL APPROACH;
MINI/MICRO-CHANNELS; VERTICAL TUBES; PIPE CHILLDOWN; 2-PHASE FLOW;
GRAVITY
AB This paper presents a comparison between experimental results from recent liquid hydrogen (LH2) transfer line chilldown experiments at high Reynolds (Re) numbers versus liquid nitrogen (LN2) experiments conducted at low Re numbers. Parasitic heat leak, inner wall temperatures, inner wall heat fluxes, and heat transfer coefficients are computed to compare between the two systems. Analysis of temperature traces and flow visualization indicates that the chilldown process evolves much more rapidly at higher Re numbers due to a quick transition from vapor flow to annular liquid flow and near immediate liquid contact along the pipe walls. The lower kinematic viscosity and surface tension of LH2, along with reduced parasitic heat leak and higher Re numbers relative to the LN2 experiments, causes chilldown to proceed almost immediately into the nucleate boiling regime, in comparison to low Re flows where >75% of the chilldown is spent in vapor film boiling. Published by Elsevier Ltd.
C1 [Hartwig, Jason] NASA, Glenn Res Ctr, Prop & Propellants Branch, Cleveland, OH 44135 USA.
[Hu, Hong; Chung, J. N.] Univ Florida, Mech & Aerosp Engn, Gainesville, FL 32611 USA.
[Styborski, Jeremy] Turbine Durabil, Hot Sect Engn Pratt & Whitney, E Hartford, CT 06118 USA.
RP Hartwig, J (reprint author), NASA, Glenn Res Ctr, Prop & Propellants Branch, Cleveland, OH 44135 USA.
EM Jason.W.Hartwig@nasa.gov
NR 45
TC 4
Z9 4
U1 5
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0017-9310
EI 1879-2189
J9 INT J HEAT MASS TRAN
JI Int. J. Heat Mass Transf.
PD SEP
PY 2015
VL 88
BP 662
EP 673
DI 10.1016/j.ijheatmasstransfer.2015.04.102
PG 12
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA CW2DZ
UT WOS:000364802600066
ER
PT J
AU Lillis, RJ
Dufek, J
Kiefer, WS
Black, BA
Manga, M
Richardson, JA
Bleacher, JE
AF Lillis, Robert J.
Dufek, Josef
Kiefer, Walter S.
Black, Benjamin A.
Manga, Michael
Richardson, Jacob A.
Bleacher, Jacob E.
TI The Syrtis Major volcano, Mars: A multidisciplinary approach to
interpreting its magmatic evolution and structural development
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID PRESSURE HYDROUS CONDITIONS; MARTIAN MANTLE CONVECTION; THARSIS
PROVINCE; THERMAL DEMAGNETIZATION; HIGH-TEMPERATURE; CRUST; HISTORY;
DYNAMO; REGION; VENUS
AB Very weak crustal magnetic fields over the Syrtis Major volcanic complex imply almost total thermal demagnetization via magmatic intrusions over a large area less than similar to 4 Ga. We fit a model of these intrusions and the resulting thermal demagnetization to maps of crustal magnetic field strength at 185 km altitude. The best fits are most consistent with a "dog bone"-shaped region of intrusive material, elongated approximately north-south, with an area of similar to 350,000 km(2) and an inferred volume of similar to 4-19 x 10(6) km(3). Such a large volume is best explained by a long-lived mantle plume beneath the Syrtis edifice. A free-air gravity anomaly high over the Syrtis Major caldera is consistent with dense mafic residue remaining at depth following crystal fractionation that produced the silicic magmas seen at the surface. The elongation of this region is consistent with ascent and north-south emplacement of magma enabled by structures parallel to and associated with the preexisting Isidis impact basin.
C1 [Lillis, Robert J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Dufek, Josef] Georgia Tech Dept Earth & Space Sci, Atlanta, GA USA.
[Kiefer, Walter S.] Lunar & Planetary Inst, Houston, TX USA.
[Black, Benjamin A.; Manga, Michael] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Richardson, Jacob A.] Univ S Florida, Sch Geosci, Tampa, FL USA.
[Bleacher, Jacob E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lillis, RJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM rlillis@ssl.Berkeley.edu
RI Bleacher, Jacob/D-1051-2012; Lillis, Robert/A-3281-2008;
OI Bleacher, Jacob/0000-0002-8499-4828; Lillis, Robert/0000-0003-0578-517X;
Kiefer, Walter/0000-0001-6741-5460; Manga, Michael/0000-0003-3286-4682
FU NASA MFRP grant [NNX09AN18G, NASA MDAP NNX11AI85G]; National Science
Foundation FESD program, NSF [EAR-1135382]; NASA grant [MDAP
NNX14AN02G]; NASA Cooperative Agreement [NNX08AC28A]; NASA MFRP
[NNX09AN18G]
FX Lillis' and Manga's work was supported by NASA MFRP grant NNX09AN18G and
NASA MDAP NNX11AI85G. Black's work was supported by the National Science
Foundation FESD program, NSF EAR-1135382. Richardson's and Bleacher's
work was supported by NASA grant MDAP NNX14AN02G. Kiefer's work at the
Lunar and Planetary Institute was supported by NASA Cooperative
Agreement NNX08AC28A. Dufek's work was supported by NASA MFRP grant
NNX09AN18G.
NR 91
TC 1
Z9 1
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD SEP
PY 2015
VL 120
IS 9
BP 1476
EP 1496
DI 10.1002/2014JE004774
PG 21
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CW1YO
UT WOS:000364788300002
ER
PT J
AU Hayne, PO
Aharonson, O
AF Hayne, P. O.
Aharonson, O.
TI Thermal stability of ice on Ceres with rough topography
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID LUNAR RADIOMETER OBSERVATIONS; SCALE TOPOGRAPHY; WATER ICE; SURFACE;
MERCURY; CRATERS; MOON; TEMPERATURES; ASTEROIDS; REGOLITH
AB The dwarf planet Ceres may have an ice-rich crust, and subsurface ice exposed by impacts or endogenic activity would be subject to sublimation. We model surface and subsurface temperatures on Ceres to assess lifetimes of water ice and other volatiles. Topographic shadowing allows a small but nonnegligible fraction (similar to 0.4%) of Ceres' surface to be perennially below the similar to 110 K criterion for 1 Gyr of stability. These areas are found above 60 degrees latitude. Other molecules (CH3OH, NH3, SO2, and CO2) may be cold trapped in smaller abundances. A model for the transport, gravitational escape, and photoionization of H2O molecules suggests net accumulation in the cold traps. Buried ice is stable within a meter for > 1 Gyr at latitudes higher than similar to 50 degrees. An illuminated polar cap of water ice would be stable within a few degrees of the poles only if it maintained a high albedo (>0.5) at present obliquity. If the obliquity exceeded 5 degrees in the geologically recent past, then a putative polar cap would have been erased. At latitudes 0 degrees-30 degrees, ice is stable under solar illumination only briefly (similar to 10-100 years), unless it has high albedo and thermal inertia, in which case lifetimes of > 10(4) years are possible. Finally, a small hemispheric asymmetry exists due to the timing of Ceres' perihelion passage, which would lead to a detectable enhancement of ice in the northern hemisphere if the orbital elements vary slowly relative to the ice accumulation rate. Our model results are potentially testable during the Dawn science mission.
C1 [Hayne, P. O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hayne, P. O.; Aharonson, O.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Aharonson, O.] Weizmann Inst Sci, Helen Kimmel Ctr Planetary Sci, IL-76100 Rehovot, Israel.
RP Hayne, PO (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Paul.O.Hayne@jpl.nasa.gov
FU Weizmann Institute of Science (WIS); Helen Kimmel Center for Planetary
Science; WIS Minerva Center; ISF I-CORE program
FX We thank Norbert Schorghofer, Bruce Bills, and Nicolas Rambaux for
valuable discussions. Mikhail Kreslavsky and Matthew Siegler provided
exceptionally thoughtful reviews, from which the paper benefited
immensely. A workshop hosted by Thomas McCord and Julie Castillo-Rogez
at the Bear Fight Institute provided the initial inspiration for this
study, which was fueled by continued workshops and support from the
Weizmann Institute of Science (WIS). Oded Aharonson wishes to
acknowledge important support from the Helen Kimmel Center for Planetary
Science, the WIS Minerva Center, and ISF I-CORE program. Part of this
work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. Copyright 2015, all rights reserved. The
source code and input files for the models used in this study are
available from the authors upon request (Paul.O.Hayne@jpl.nasa.gov),
pending approval for public release by NASA/JPL.
NR 53
TC 10
Z9 10
U1 4
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD SEP
PY 2015
VL 120
IS 9
BP 1567
EP 1584
DI 10.1002/2015JE004887
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CW1YO
UT WOS:000364788300007
ER
PT J
AU Eldridge, JI
Chambers, MD
AF Eldridge, Jeffrey I.
Chambers, Matthew D.
TI Fiber optic thermometer using Cr-doped GdAlO3 broadband emission decay
SO MEASUREMENT SCIENCE and TECHNOLOGY
LA English
DT Article
DE luminescence; thermometer; thermographic phosphor
ID TEMPERATURE SENSOR; FLUORESCENCE LIFETIME; CRYSTAL FIBER; YAG CRYSTAL;
LUMINESCENCE; DEPENDENCES; SYSTEM; PROBES; HEAD
AB Luminescence decay temperature measurements are performed from 800 to 1200 degrees C using a Cr-doped GdAlO3 (Cr:GdAlO3) sensor tip on a YAG single crystal fiber. As a thermographic phosphor, Cr:GdAlO3 combines the intense luminescence of transition metal dopants with the high temperature long decay times usually exhibited only by rare earth dopants. The proposed mechanism is emission by the Cr3+ dopant via the spin-allowed T-4(2) -> (4)A(2) transition supported by a reservoir state in E-2 which populates T-4(2) (E-2 -> T-4(2) 4 2) through thermal equilibration. The relative energy levels and transition probabilities associated with the strong crystal field at the Al3+ site in the perovskite structure of GdAlO3 are favorable for suppressing thermal quenching of luminescence. Results from a single-fiber configuration sensor, based on a YAG fiber for its low background luminescence, are presented. Using a decay curve fitting procedure that accounts for background fluorescence, accuracies of better than +/- 5 degrees C are demonstrated.
C1 [Eldridge, Jeffrey I.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Eldridge, JI (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM jeffrey.i.eldridge@nasa.gov
FU Aeronautics Research Directorate Seedling Fund part of the NASA
Fundamental Aeronautics Program; Aeronautical Sciences Project part of
the NASA Fundamental Aeronautics Program
FX The authors gratefully acknowledge the support of the Aeronautics
Research Directorate Seedling Fund and the Aeronautical Sciences
Project, both part of the NASA Fundamental Aeronautics Program.
NR 34
TC 3
Z9 3
U1 6
U2 19
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 SEP
PY 2015
VL 26
IS 9
AR 095202
DI 10.1088/0957-0233/26/9/095202
PG 12
WC Engineering, Multidisciplinary; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA CV5RQ
UT WOS:000364329200026
ER
PT J
AU Oberg, J
AF Oberg, James
TI on Russian space Stuck in decline
SO AEROSPACE AMERICA
LA English
DT Article
C1 [Oberg, James] NASA, New York, NY USA.
EM jameseoberg@comcast.net
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0740-722X
J9 AEROSPACE AM
JI Aerosp. Am.
PD SEP
PY 2015
VL 53
IS 8
BP 21
EP +
PG 4
WC Engineering, Aerospace
SC Engineering
GA CV5LM
UT WOS:000364312200015
ER
PT J
AU Goldstein, DA
D'Andrea, CB
Fischer, JA
Foley, RJ
Gupta, RR
Kessler, R
Kim, AG
Nichol, RC
Nugent, PE
Papadopoulos, A
Sako, M
Smith, M
Sullivan, M
Thomas, RC
Wester, W
Wolf, RC
Abdalla, FB
Banerji, M
Benoit-Levy, A
Bertin, E
Brooks, D
Rosell, AC
Castander, FJ
da Costa, LN
Covarrubias, R
DePoy, DL
Desai, S
Diehl, HT
Doel, P
Eifler, TF
Neto, AF
Finley, DA
Flaugher, B
Fosalba, P
Frieman, J
Gerdes, D
Gruen, D
Gruendl, RA
James, D
Kuehn, K
Kuropatkin, N
Lahav, O
Li, TS
Maia, MAG
Makler, M
March, M
Marshall, JL
Martini, P
Merritt, KW
Miquel, R
Nord, B
Ogando, R
Plazas, AA
Romer, AK
Roodman, A
Sanchez, E
Scarpine, V
Schubnell, M
Sevilla-Noarbe, I
Smith, RC
Soares-Santos, M
Sobreira, F
Suchyta, E
Swanson, MEC
Tarle, G
Thaler, J
Walker, AR
AF Goldstein, D. A.
D'Andrea, C. B.
Fischer, J. A.
Foley, R. J.
Gupta, R. R.
Kessler, R.
Kim, A. G.
Nichol, R. C.
Nugent, P. E.
Papadopoulos, A.
Sako, M.
Smith, M.
Sullivan, M.
Thomas, R. C.
Wester, W.
Wolf, R. C.
Abdalla, F. B.
Banerji, M.
Benoit-Levy, A.
Bertin, E.
Brooks, D.
Rosell, A. Carnero
Castander, F. J.
da Costa, L. N.
Covarrubias, R.
DePoy, D. L.
Desai, S.
Diehl, H. T.
Doel, P.
Eifler, T. F.
Neto, A. Fausti
Finley, D. A.
Flaugher, B.
Fosalba, P.
Frieman, J.
Gerdes, D.
Gruen, D.
Gruendl, R. A.
James, D.
Kuehn, K.
Kuropatkin, N.
Lahav, O.
Li, T. S.
Maia, M. A. G.
Makler, M.
March, M.
Marshall, J. L.
Martini, P.
Merritt, K. W.
Miquel, R.
Nord, B.
Ogando, R.
Plazas, A. A.
Romer, A. K.
Roodman, A.
Sanchez, E.
Scarpine, V.
Schubnell, M.
Sevilla-Noarbe, I.
Smith, R. C.
Soares-Santos, M.
Sobreira, F.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Thaler, J.
Walker, A. R.
TI AUTOMATED TRANSIENT IDENTIFICATION IN THE DARK ENERGY SURVEY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE methods: data analysis; methods: statistical; supernovae: general
ID II SUPERNOVA SURVEY; VARIABLE-STARS; IA SUPERNOVAE; WIDE-FIELD;
CLASSIFICATION; SEARCH; DISCOVERY; CONSTRAINTS; SOFTWARE; CAMERA
AB We describe an algorithm for identifying point-source transients and moving objects on reference-subtracted optical images containing artifacts of processing and instrumentation. The algorithm makes use of the supervised machine learning technique known as Random Forest. We present results from its use in the Dark Energy Survey Supernova program (DES-SN), where it was trained using a sample of 898,963 signal and background events generated by the transient detection pipeline. After reprocessing the data collected during the first DES-SN observing season (2013 September through 2014 February) using the algorithm, the number of transient candidates eligible for human scanning decreased by a factor of 13.4, while only 1.0% of the artificial Type Ia supernovae (SNe) injected into search images to monitor survey efficiency were lost, most of which were very faint events. Here we characterize the algorithm's performance in detail, and we discuss how it can inform pipeline design decisions for future time-domain imaging surveys, such as the Large Synoptic Survey Telescope and the Zwicky Transient Facility. An implementation of the algorithm and the training data used in this paper are available at http://portal.nserc.gov/project/dessn/autoscan.
C1 [Goldstein, D. A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Goldstein, D. A.; Kim, A. G.; Nugent, P. E.; Thomas, R. C.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[D'Andrea, C. B.; Nichol, R. C.; Papadopoulos, A.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Sako, M.; Wolf, R. C.; Eifler, T. F.; March, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Foley, R. J.; Gruendl, R. A.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Foley, R. J.; Thaler, J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Gupta, R. R.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Kessler, R.; Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Kessler, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Smith, M.; Sullivan, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Wester, W.; Diehl, H. T.; Finley, D. A.; Flaugher, B.; Frieman, J.; Kuropatkin, N.; Nord, B.; Scarpine, V.; Soares-Santos, M.; Sobreira, F.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Banerji, M.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England.
[Banerji, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Bertin, E.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France.
[Bertin, E.] CNRS, UMR7095, F-75014 Paris, France.
[Rosell, A. Carnero; da Costa, L. N.; Neto, A. Fausti; Maia, M. A. G.; Ogando, R.; Sobreira, F.] Lab Interinst E Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Rosell, A. Carnero; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Castander, F. J.; Fosalba, P.] IEEC CSIC, Fac Ciencies, Inst Ciencies Espai, E-08193 Barcelona, Spain.
[Covarrubias, R.; Gruendl, R. A.; Swanson, M. E. C.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[DePoy, D. L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[DePoy, D. L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Desai, S.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gerdes, D.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Gruen, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Gruen, D.] Univ Observ Munich, D-81679 Munich, Germany.
[James, D.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile.
[Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Makler, M.] Ctr Brasileiro Pesquisas Fis, ICRA, BR-22290180 Rio De Janeiro, RJ, Brazil.
[Martini, P.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Martini, P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Miquel, R.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
[Plazas, A. A.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Romer, A. K.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Roodman, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Roodman, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain.
[Suchyta, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
RP Goldstein, DA (reprint author), Univ Calif Berkeley, Dept Astron, 501 Campbell Hall 3411, Berkeley, CA 94720 USA.
RI Ogando, Ricardo/A-1747-2010; Makler, Martin/G-2639-2012; Sanchez,
Eusebio/H-5228-2015; Fosalba Vela, Pablo/I-5515-2016; Sobreira,
Flavia/F-4168-2015;
OI Ogando, Ricardo/0000-0003-2120-1154; Makler, Martin/0000-0003-2206-2651;
Sanchez, Eusebio/0000-0002-9646-8198; Sobreira,
Flavia/0000-0002-7822-0658; Suchyta, Eric/0000-0002-7047-9358; Banerji,
Manda/0000-0002-0639-5141; Goldstein, Daniel/0000-0003-3461-8661;
Abdalla, Filipe/0000-0003-2063-4345; Sullivan, Mark/0000-0001-9053-4820
FU U.S. Department of Energy; U.S. National Science Foundation; Ministry of
Science and Education of Spain; Science and Technology Facilities
Council of the United Kingdom; Higher Education Funding Council for
England; National Center for Supercomputing Applications at the
University of Illinois at Urbana-Champaign; Kavli Institute of
Cosmological Physics at the University of Chicago; Financiadora de
Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do
Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento
Cientifico e Tecnologico and the Ministerio da Ciencia e Tecnologia;
Deutsche Forschungsgemeinschaft; Office of Science of the U.S.
Department of Energy [DE-AC02-05CH11231]; PAPDRJ CAPES/FAPERJ
Fellowship; CAPES [3171-13-2]; MINECO [AYA2012-39559, ESP2013-48274,
FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234];
European Union
FX D.A.G. thanks Josh Bloom for productive conversations and an anonymous
referee for comments that improved the paper. We are grateful for the
extraordinary contributions of our CTIO colleagues and the DES Camera,
Commissioning and Science Verification teams for achieving excellent
instrument and telescope conditions that have made this work possible.
The success of this project also relies critically on the expertise and
dedication of the DES Data Management organization. Funding for DES
projects has been provided by the U.S. Department of Energy, the U.S.
National Science Foundation, the Ministry of Science and Education of
Spain, the Science and Technology Facilities Council of the United
Kingdom, the Higher Education Funding Council for England, the National
Center for Supercomputing Applications at the University of Illinois at
Urbana-Champaign, the Kavli Institute of Cosmological Physics at the
University of Chicago, Financiadora de Estudos e Projetos, Fundacao
Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro,
Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the
Ministerio da Ciencia e Tecnologia, the Deutsche Forschungsgemeinschaft,
and the collaborating institutions in the Dark Energy Survey. The
collaborating institutions are Argonne National Laboratory, the
University of California, Santa Cruz, the University of Cambridge,
Centro de Investigaciones Energeticas, Medioambientales y
Tecnologicas-Madrid, the University of Chicago, University College
London, the DES-Brazil Consortium, the Eidgenossische Tecnische
Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the
University of Edinburgh, the University of Illinois at Urbana-Champaign,
the Institut de Ciencies de l'Espai (IEEC/CSIC), the Intitut de Fisica
d'Altes Energies, Lawrence Berkeley National Laboratory, the
Ludwig-Maximilians Universitat and the associated Excellence Cluster
Universe, the University of Michigan, the National Optical Astronomy
Observatory, the University of Nottingham, the Ohio State University,
the University of Pennsylvania, the University of Portsmouth, SLAC
National Acclerator Laboratory, Stanford University, the University of
Sussex, and Texas A&M University. This research used resources of the
National Energy Research Scientific Computing Center, a DOE Office of
Science User Facility supported by the Office of Science of the U.S.
Department of Energy under Contract No. DE-AC02-05CH11231. Figure 4 was
generated with a modified version of triangle.py (Foreman-Mackey et al.
2014). A.C.R. acknowledges financial support provided by the PAPDRJ
CAPES/FAPERJ Fellowship. F.S. acknowledges financial support provided by
CAPES under contract No. 3171-13-2. The DES participants from Spanish
institutions are partially supported by MINECO under grants
AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia
Severo Ochoa SEV-2012-0234, some of which include ERDF funds from the
European Union.
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JI Astron. J.
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DI 10.1088/0004-6256/150/3/82
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CV1IR
UT WOS:000364008100018
ER
PT J
AU Rich, EA
Wisniewski, JP
Mayama, S
Brandt, TD
Hashimoto, J
Kudo, T
Kusakabe, N
Espaillat, C
Abe, L
Akiyama, E
Brandner, W
Carson, JC
Currie, T
Egner, S
Feldt, M
Follette, K
Goto, M
Grady, CA
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, SS
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, GR
Kuzuhara, M
Kwon, J
Matsuo, T
McElwain, MW
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Qi, CH
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, YH
Takami, M
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Rich, Evan A.
Wisniewski, John P.
Mayama, Satoshi
Brandt, Timothy D.
Hashimoto, Jun
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Espaillat, Catherine
Abe, Lyu
Akiyama, Eiji
Brandner, Wolfgang
Carson, Joseph C.
Currie, Thayne
Egner, Sebastian
Feldt, Markus
Follette, Kate
Goto, Miwa
Grady, Carol A.
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko S.
Henning, Thomas
Hodapp, Klaus W.
Ishii, Miki
Iye, Masanori
Janson, Markus
Kandori, Ryo
Knapp, Gillian R.
Kuzuhara, Masayuki
Kwon, Jungmi
Matsuo, Taro
McElwain, Michael W.
Miyama, Shoken
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishimura, Tetsuo
Pyo, Tae-Soo
Qi, Chunhua
Serabyn, Eugene
Suenaga, Takuya
Suto, Hiroshi
Suzuki, Ryuji
Takahashi, Yasuhiro H.
Takami, Michihiro
Takato, Naruhisa
Terada, Hiroshi
Thalmann, Christian
Tomono, Daigo
Turner, Edwin L.
Watanabe, Makoto
Yamada, Toru
Takami, Hideki
Usuda, Tomonori
Tamura, Motohide
TI NEAR-IR POLARIZED SCATTERED LIGHT IMAGERY OF THE DoAr 28 TRANSITIONAL
DISK
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE protoplanetary disks; stars: variables: T Tauri, Herbig Ae/Be
ID PROTOPLANETARY DISKS; RADIATIVE-TRANSFER; PLANET FORMATION;
RHO-OPHIUCHI; SIZE DISTRIBUTION; BROWN DWARFS; STAR CLUSTER; ORION
NEBULA; DARK CLOUD; LKCA 15
AB We present the first spatially resolved polarized scattered light H-band detection of the DoAr 28 transitional disk. Our two epochs of imagery detect the scattered light disk from our effective inner working angle of 0".10 (13 AU) out to 0".50 (65 AU). This inner working angle is interior to the location of the system's gap inferred by previous studies using spectral energy distribution modeling (15 AU). We detected a candidate point source companion 1".08 northwest of the system; however, our second epoch of imagery strongly suggests that this object is a background star. We constructed a grid of Monte Carlo Radiative Transfer models of the system, and our best fit models utilize a modestly inclined (50 degrees), 0.01 M-circle dot disk that has a partially depleted inner gap from the dust sublimation radius out to similar to 8 AU. Subtracting this best fit, axi-symmetric model from our polarized intensity data reveals evidence for two small asymmetries in the disk, which could be attributable to a variety of mechanisms.
C1 [Rich, Evan A.; Wisniewski, John P.; Hashimoto, Jun] Univ Oklahoma, Homer L Dodge Dept Phys, Norman, OK 73071 USA.
[Mayama, Satoshi] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan.
[Brandt, Timothy D.; Turner, Edwin L.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA.
[Kudo, Tomoyuki; Currie, Thayne; Egner, Sebastian; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko S.; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Kusakabe, Nobuhiko; Akiyama, Eiji; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Suto, Hiroshi; Suzuki, Ryuji; Takami, Hideki; Usuda, Tomonori; Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Espaillat, Catherine] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR 7293, F-06108 Nice 2, France.
[Brandner, Wolfgang; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Carson, Joseph C.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Follette, Kate] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Goto, Miwa] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Grady, Carol A.; McElwain, Michael W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Grady, Carol A.] Eureka Sci, Oakland, CA 96002 USA.
[Grady, Carol A.] Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Janson, Markus] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, SE-10691 Stockholm, Sweden.
[Knapp, Gillian R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Kwon, Jungmi; Takahashi, Yasuhiro H.; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto, Kyoto 6068502, Japan.
[Miyama, Shoken] Hiroshima Univ, Higashihiroshima, Hiroshima 7398511, Japan.
[Moro-Martin, Amaya] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Moro-Martin, Amaya] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA.
[Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Suenaga, Takuya] Grad Univ Adv Studies, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
[Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Thalmann, Christian] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Rich, EA (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys, Norman, OK 73071 USA.
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016;
OI Watanabe, Makoto/0000-0002-3656-4081; Feldt, Markus/0000-0002-4188-5242
FU NSF-AST [1009203, 1008440, 1009314]; NASA Origins of Solar System
program [NNX13AK17G, RTOP 12-OSS12-0045, NNG13PB64P]; MEXT Japan;
Mitsubishi Foundation; NASA Exoplanet Science Institute; NASA through
the Sagan Fellowship Program
FX We thank the referee for providing suggestions that improved the content
and layout of this paper. We acknowledge support from NSF-AST 1009203
(J.C.), 1008440 (C.G.), and 1009314 (E.R., J.W., J.H.) and the NASA
Origins of Solar System program under NNX13AK17G (J. W.), RTOP
12-OSS12-0045 (M.M.), and NNG13PB64P (C.G.). This work is partly
supported by a Grant-in-Aid for Science Research in a Priority Area from
MEXT Japan and by the Mitsubishi Foundation. This work was performed [in
part] under contract with the Jet Propulsion Laboratory (JPL) funded by
NASA through the Sagan Fellowship Program executed by the NASA Exoplanet
Science Institute. The authors recognize and acknowledge the significant
cultural role and reverence that the summit of Mauna Kea has always had
within the indigenous Hawaiian community. We are most fortunate to have
the opportunity to conduct observations from this mountain.
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UT WOS:000364008100023
ER
PT J
AU Friedman, AS
Wood-Vasey, WM
Marion, GH
Challis, P
Mandel, KS
Bloom, JS
Modjaz, M
Narayan, G
Hicken, M
Foley, RJ
Klein, CR
Starr, DL
Morgan, A
Rest, A
Blake, CH
Miller, AA
Falco, EE
Wyatt, WF
Mink, J
Skrutskie, MF
Kirshner, RP
AF Friedman, Andrew S.
Wood-Vasey, W. M.
Marion, G. H.
Challis, Peter
Mandel, Kaisey S.
Bloom, Joshua S.
Modjaz, Maryam
Narayan, Gautham
Hicken, Malcolm
Foley, Ryan J.
Klein, Christopher R.
Starr, Dan L.
Morgan, Adam
Rest, Armin
Blake, Cullen H.
Miller, Adam A.
Falco, Emilio E.
Wyatt, William F.
Mink, Jessica
Skrutskie, Michael F.
Kirshner, Robert P.
TI CFAIR2: NEAR-INFRARED LIGHT CURVES OF 94 TYPE Ia SUPERNOVAE
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmology: observations; distance scale; infrared: stars; supernovae:
general; techniques: image processing; techniques: photometric
ID HUBBLE-SPACE-TELESCOPE; 2MASS CALIBRATION FIELDS; CORE-COLLAPSE
SUPERNOVAE; DARK ENERGY CONSTRAINTS; PHOTOMETRY DATA RELEASE; SN 2005HK;
COSMOLOGICAL CONSTRAINTS; LEGACY SURVEY; DECLINE-RATE; HOST GALAXY
AB CfAIR2 is a large, homogeneously reduced set of near-infrared (NIR) light curves (LCs) for Type Ia supernovae (SNe Ia) obtained with the 1.3 m Peters Automated InfraRed Imaging TELescope. This data set includes 4637 measurements of 94 SNe Ia and 4 additional SNe Iax observed from 2005 to 2011 at the Fred Lawrence Whipple Observatory on Mount Hopkins, Arizona. CfAIR2 includes JHKs photometric measurements for 88 normal and 6 spectroscopically peculiar SN Ia in the nearby universe, with a median redshift of z similar to 0.021 for the normal SN Ia. CfAIR2 data span the range from -13 days to +127 days from B-band maximum. More than half of the LCs begin before the time of maximum, and the coverage typically contains similar to 13-18 epochs of observation, depending on the filter. We present extensive tests that verify the fidelity of the CfAIR2 data pipeline, including comparison to the excellent data of the Carnegie Supernova Project. CfAIR2 contributes to a firm local anchor for SN cosmology studies in the NIR. Because SN Ia are more nearly standard candles in the NIR and are less vulnerable to the vexing problems of extinction by dust, CfAIR2 will help the SN cosmology community develop more precise and accurate extragalactic distance probes to improve our knowledge of cosmological parameters, including dark energy and its potential time variation.
C1 [Friedman, Andrew S.; Marion, G. H.; Challis, Peter; Mandel, Kaisey S.; Narayan, Gautham; Hicken, Malcolm; Falco, Emilio E.; Wyatt, William F.; Mink, Jessica; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Friedman, Andrew S.] MIT, Ctr Theoret Phys, Cambridge, MA 02139 USA.
[Friedman, Andrew S.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Bloom, Joshua S.; Klein, Christopher R.; Starr, Dan L.; Morgan, Adam] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Modjaz, Maryam] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Narayan, Gautham] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Narayan, Gautham] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Foley, Ryan J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Foley, Ryan J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Rest, Armin] Space Telescope Sci Inst, STScI, Baltimore, MD 21218 USA.
[Blake, Cullen H.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Miller, Adam A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Skrutskie, Michael F.] Dept Astron, Charlottesville, VA 22904 USA.
RP Friedman, AS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM asf@mit.edu; wmwv@pitt.edu; hman@astro.as.utexas.edu;
pchallis@cfa.harvard.edu; kmandel@cfa.harvard.edu;
joshbloom@berkeley.edu; mmodjaz@nyu.edu; gnarayan@noao.edu;
malcolmhicken@hotmail.com; rfoley@illinois.edu; cklein@berkeley.edu;
dstarr1@gmail.com; amorgan@astro.berkeley.edu; arest@stsci.edu;
chblake@sas.upenn.edu; amiller@astro.caltech.edu;
efalco@cfa.harvard.edu; wfw781kra@gmail.com; jmink@cfa.harvard.edu;
skrutskie@virginia.edu; rkirshner@cfa.harvard.edu
RI Friedman, Andrew/I-4691-2013;
OI Friedman, Andrew/0000-0003-1334-039X; Mink, Jessica/0000-0003-3594-1823;
Narayan, Gautham/0000-0001-6022-0484
FU Harvard University Milton Fund; National Aeronautics and Space
Administration (NASA) [NNG06GH50G]; DOE SciDAC grant
[DE-FC02-06ER41453]; Sloan Research Fellowship; NASA [NNX13AC58G,
NAS5-26555, NAS 5-26555, HST-HF-51325.01]; U.S. National Science
Foundation (NSF); NSF STS Postdoctoral Fellowship [SES-1056580]; U.S.
National Science Foundation [AST-057475]; NSF [AST 12-11196, AST
09-097303, AST 06-06772, PHY05-51164, AST-1352405]; Miller Institute at
UC Berkeley; STScI [HST-HF-51277.01-A]; Harvard Origins of Life
Initiative; Optical and Infrared Astronomy Division of the CfA; Harvard
FAS Science Division Research Computing Group
FX The Peters Automated Infrared Imaging TElescope (PAIRITEL) is operated
by the Smithsonian Astrophysical Observatory (SAO) and was enabled by a
grant from the Harvard University Milton Fund, the camera loan from the
University of Virginia, and continued support of the SAO and UC
Berkeley. Partial support for PAIRITEL operations and this work comes
from National Aeronautics and Space Administration (NASA) Swift Guest
Investigator grant NNG06GH50G ("PAIRITEL: Infrared Follow-up for Swift
Transients"). PAIRITEL support and processing are conducted under the
auspices of a DOE SciDAC grant (DE-FC02-06ER41453), which provides
support to J.S.B.'s group. J.S.B. thanks the Sloan Research Fellowship
for partial support, as well as NASA grant NNX13AC58G. We gratefully
made use of the NASA/IPAC Extragalactic Database (NED). The NASA/IPAC
Extragalactic Database (NED) is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA. This publication makes use of data products from 2MASS, funded by
NASA and the U.S. National Science Foundation (NSF). IAUC/CBET were very
useful. A.S.F. acknowledges support from an NSF STS Postdoctoral
Fellowship (SES-1056580), an NSF Graduate Research Fellowship, and a
NASA Graduate Research Program Fellowship. M.W.V. is funded by a grant
from the U.S. National Science Foundation (AST-057475). R.P.K.
acknowledges NSF Grants AST 12-11196, AST 09-097303, and AST 06-06772.
M.M. acknowledges support in part from the Miller Institute at UC
Berkeley, from Hubble Fellowship grant HST-HF-51277.01-A, awarded by
STScI, which is operated by AURA under NASA contract NAS5-26555, and
from the NSF CAREER award AST-1352405. A.A.M. acknowledges support for
this work by NASA from a Hubble Fellowship grant HST-HF-51325.01,
awarded by STScI, operated by AURA, Inc., for NASA, under contract NAS
5-26555. Part of the research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. A.S.F., R.P.K., and
M.M. thank the Kavli Institute for Theoretical Physics at UC Santa
Barbara, which is supported by the NSF through grant PHY05-51164. C.B.
acknowledges support from the Harvard Origins of Life Initiative.
Computations in this work were run on machines supported by the Harvard
Astronomy Computation Facility, including the CfA Hydra cluster and
machines supported by the Optical and Infrared Astronomy Division of the
CfA. Other crucial computations were performed on the Harvard Odyssey
cluster, supported by the Harvard FAS Science Division Research
Computing Group. We thank the anonymous referee for a thorough and fair
report that significantly helped to improve the paper.
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SC Astronomy & Astrophysics
GA CV1WX
UT WOS:000364049900009
ER
PT J
AU Madsen, KK
Harrison, FA
Markwardt, CB
An, H
Grefenstette, BW
Bachetti, M
Miyasaka, H
Kitaguchi, T
Bhalerao, V
Boggs, S
Christensen, FE
Craig, WW
Forster, K
Fuerst, F
Hailey, CJ
Perri, M
Puccetti, S
Rana, V
Stern, D
Walton, DJ
Westergaard, NJ
Zhang, WW
AF Madsen, Kristin K.
Harrison, Fiona A.
Markwardt, Craig B.
An, Hongjun
Grefenstette, Brian W.
Bachetti, Matteo
Miyasaka, Hiromasa
Kitaguchi, Takao
Bhalerao, Varun
Boggs, Steve
Christensen, Finn E.
Craig, William W.
Forster, Karl
Fuerst, Felix
Hailey, Charles J.
Perri, Matteo
Puccetti, Simonetta
Rana, Vikram
Stern, Daniel
Walton, Dominic J.
Westergaard, Niels Jorgen
Zhang, William W.
TI CALIBRATION OF THE NuSTAR HIGH-ENERGY FOCUSING X-RAY TELESCOPE
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE instrumentation: detectors; space vehicles: instruments; telescopes
ID XMM-NEWTON; CROSS-CALIBRATION; CRAB PULSAR; MISSION; SWIFT; EMISSION;
CHANDRA; SUZAKU; RXTE; X-1
AB We present the calibration of the Nuclear Spectroscopic Telescope Array (NuSTAR) X-ray satellite. We used the Crab as the primary effective area calibrator and constructed a piece-wise linear spline function to modify the vignetting response. The achieved residuals for all off-axis angles and energies, compared to the assumed spectrum, are typically better than +/- 2% up to 40 keV and 5%-10% above due to limited counting statistics. An empirical adjustment to the theoretical two-dimensional point-spread function (PSF) was found using several strong point sources, and no increase of the PSF half-power diameter has been observed since the beginning of the mission. We report on the detector gain calibration, good to 60 eV for all grades, and discuss the timing capabilities of the observatory, which has an absolute timing of +/- 3 ms. Finally, we present cross-calibration results from two campaigns between all the major concurrent X-ray observatories (Chandra, Swift, Suzaku, and XMM-Newton), conducted in 2012 and 2013 on the sources 3C 273 and PKS 2155-304, and show that the differences in measured flux is within similar to 10% for all instruments with respect to NuSTAR.
C1 [Madsen, Kristin K.; Harrison, Fiona A.; Grefenstette, Brian W.; Miyasaka, Hiromasa; Forster, Karl; Fuerst, Felix; Rana, Vikram; Walton, Dominic J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Markwardt, Craig B.; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[An, Hongjun] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Bachetti, Matteo] Univ Toulouse, Toulouse, France.
[Bachetti, Matteo] UPS OMP, Toulouse, France.
[Bachetti, Matteo] IRAP, Toulouse, France.
[Bachetti, Matteo] CNRS, F-31028 Toulouse 4, France.
[Bachetti, Matteo] Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France.
[Bachetti, Matteo] Osservatorio Astron Cagliari, Cagliari, Italy.
[Kitaguchi, Takao] RIKEN, Wako, Saitama 3510198, Japan.
[Bhalerao, Varun] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Boggs, Steve; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, Finn E.; Westergaard, Niels Jorgen] 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.
[Perri, Matteo; Puccetti, Simonetta] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Stern, Daniel; Walton, Dominic J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Madsen, KK (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RI Boggs, Steven/E-4170-2015;
OI Boggs, Steven/0000-0001-9567-4224; Bhalerao, Varun/0000-0002-6112-7609;
Puccetti, Simonetta/0000-0002-2734-7835; Bachetti,
Matteo/0000-0002-4576-9337; Madsen, Kristin/0000-0003-1252-4891
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration
FX We would like to thank the referee for helpful comments and suggestions
which helped improve the paper. 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).
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PT J
AU Torre, G
Schwartz, RA
Benvenuto, F
Massone, AM
Piana, M
AF Torre, G.
Schwartz, R. A.
Benvenuto, F.
Massone, A. M.
Piana, M.
TI Inverse diffraction for the Atmospheric Imaging Assembly in the Solar
Dynamics Observatory
SO INVERSE PROBLEMS
LA English
DT Article
DE Solar Dynamics Observatory; inverse diffraction; astronomical imaging;
expectation maximization
ID RHESSI; SDO
AB The Atmospheric Imaging Assembly in the Solar Dynamics Observatory provides full Sun images every 12 s in each of 7 extreme ultraviolet passbands. However, for a significant amount of these images, saturation affects their most intense core, preventing scientists from a full exploitation of their physical meaning. In this paper we describe a mathematical and automatic procedure for the recovery of information in the primary saturation region based on a correlation/inversion analysis of the diffraction pattern associated to the telescope observations. Further, we suggest an interpolation-based method for determining the image background that allows the recovery of information also in the region of secondary saturation (blooming).
C1 [Torre, G.; Piana, M.] Univ Genoa, Dipartimento Matemat, I-16146 Genoa, Italy.
[Schwartz, R. A.] Catholic Univ Amer, Greenbelt, MD 20771 USA.
[Schwartz, R. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Benvenuto, F.] Ecole Polytech, CMAP, F-91128 Palaiseau, France.
[Massone, A. M.; Piana, M.] CNR SPIN Genova, I-16146 Genoa, Italy.
RP Torre, G (reprint author), Univ Genoa, Dipartimento Matemat, Via Dodecaneso 35, I-16146 Genoa, Italy.
EM piana@dima.unige.it
RI piana, michele/H-9376-2015;
OI PIANA, MICHELE/0000-0003-1700-991X
FU Italian INdAM-GNCS; NASA [NNX14AG06G]; European Union Seventh Framework
Programme (FP7) [246016]
FX This work was supported by a grant of the Italian INdAM-GNCS and by the
NASA grant NNX14AG06G. Federico Benvenuto carried out this work during
the tenure of an ERCIM 'Alain Bensoussan' Fellowship Programme. The
research leading to these results has received funding from the European
Union Seventh Framework Programme (FP7/2007-2013) under grant agreement
n 246016.
NR 17
TC 1
Z9 1
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0266-5611
EI 1361-6420
J9 INVERSE PROBL
JI Inverse Probl.
PD SEP
PY 2015
VL 31
IS 9
AR 095006
DI 10.1088/0266-5611/31/9/095006
PG 17
WC Mathematics, Applied; Physics, Mathematical
SC Mathematics; Physics
GA CV3DF
UT WOS:000364137900007
ER
PT J
AU Jaynes, AN
Baker, DN
Singer, HJ
Rodriguez, JV
Loto'aniu, TM
Ali, AF
Elkington, SR
Li, X
Kanekal, SG
Claudepierre, SG
Fennell, JF
Li, W
Thorne, RM
Kletzing, CA
Spence, HE
Reeves, GD
AF Jaynes, A. N.
Baker, D. N.
Singer, H. J.
Rodriguez, J. V.
Loto'aniu, T. M.
Ali, A. F.
Elkington, S. R.
Li, X.
Kanekal, S. G.
Claudepierre, S. G.
Fennell, J. F.
Li, W.
Thorne, R. M.
Kletzing, C. A.
Spence, H. E.
Reeves, G. D.
TI Source and seed populations for relativistic electrons: Their roles in
radiation belt changes
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE radiation belts; Van Allen Probes; relativistic electrons; VLF waves;
ULF waves; substorms
ID VAN ALLEN PROBES; PHASE-SPACE DENSITY; SOLAR-WIND; GEOMAGNETIC STORMS;
OUTER MAGNETOSPHERE; LOSS MECHANISMS; MAGNETIC-FIELD; ACCELERATION;
CHORUS; ZONE
AB Strong enhancements of outer Van Allen belt electrons have been shown to have a clear dependence on solar wind speed and on the duration of southward interplanetary magnetic field. However, individual case study analyses also have demonstrated that many geomagnetic storms produce little in the way of outer belt enhancements and, in fact, may produce substantial losses of relativistic electrons. In this study, focused upon a key period in August-September 2014, we use GOES geostationary orbit electron flux data and Van Allen Probes particle and fields data to study the process of radiation belt electron acceleration. One particular interval, 13-22 September, initiated by a short-lived geomagnetic storm and characterized by a long period of primarily northward interplanetary magnetic field (IMF), showed strong depletion of relativistic electrons (including an unprecedented observation of long-lasting depletion at geostationary orbit) while an immediately preceding, and another immediately subsequent, storm showed strong radiation belt enhancement. We demonstrate with these data that two distinct electron populations resulting from magnetospheric substorm activity are crucial elements in the ultimate acceleration of highly relativistic electrons in the outer belt: the source population (tens of keV) that give rise to VLF wave growth and the seed population (hundreds of keV) that are, in turn, accelerated through VLF wave interactions to much higher energies. ULF waves may also play a role by either inhibiting or enhancing this process through radial diffusion effects. If any components of the inner magnetospheric accelerator happen to be absent, the relativistic radiation belt enhancement fails to materialize.
C1 [Jaynes, A. N.; Baker, D. N.; Ali, A. F.; Elkington, S. R.; Li, X.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Singer, H. J.] NOAA Space Weather Predict Ctr, Boulder, CO USA.
[Rodriguez, J. V.; Loto'aniu, T. M.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Rodriguez, J. V.; Loto'aniu, T. M.] NOAA Natl Ctr Environm Informat, Boulder, CO USA.
[Kanekal, S. G.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Claudepierre, S. G.; Fennell, J. F.] Aerosp Corp, Space Sci Lab, Los Angeles, CA 90009 USA.
[Li, W.; Thorne, R. M.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Kletzing, C. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Reeves, G. D.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM USA.
RP Jaynes, AN (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
EM allison.jaynes@lasp.colorado.edu
RI Reeves, Geoffrey/E-8101-2011;
OI Reeves, Geoffrey/0000-0002-7985-8098; Ali, Ashar/0000-0003-2981-5791;
Kletzing, Craig/0000-0002-4136-3348; RODRIGUEZ, JUAN/0000-0002-6847-4136
FU RBSP-ECT through JHU/APL [967399]; NASA [NAS5-01072]
FX The research presented here was supported by RBSP-ECT funding through
JHU/APL contract 967399 (under prime NASA contract NAS5-01072). All data
used in this paper are currently available via CDAweb
(http://cdaweb.gsfc.nasa.gov/) or through the individual Van Allen
Probes instrument suite web-pages. We wish to thank S. Claudepierre of
theMagEIS teamfor providing data for this study prior to its public
release.
NR 63
TC 25
Z9 25
U1 2
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2015
VL 120
IS 9
BP 7240
EP 7254
DI 10.1002/2015JA021234
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800012
ER
PT J
AU Liu, YH
Hesse, M
Kuznetsova, M
AF Liu, Yi-Hsin
Hesse, M.
Kuznetsova, M.
TI Orientation of X lines in asymmetric magnetic reconnectionMass ratio
dependency
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE reconnection; asymmetric; magnetopause; X line orientation; bisection;
tearing
ID FLUX-TRANSFER EVENTS; MAGNETOPAUSE RECONNECTION; DAYSIDE MAGNETOPAUSE;
FIELD; SIMULATIONS; COLLISIONLESS; LOCATION; CLUSTER; PHYSICS; PLASMA
AB Using fully kinetic simulations, we study the X line orientation of magnetic reconnection in an asymmetric configuration. A spatially localized perturbation is employed to induce a single X line, which has sufficient freedom to choose its orientation in three-dimensional systems. The effect of ion to electron mass ratio is investigated, and the X line appears to bisect the magnetic shear angle across the current sheet in the large mass ratio limit. The orientation can generally be deduced by scanning through the corresponding 2-D simulations to find the reconnection plane that maximizes the peak reconnection electric field. The deviation from the bisection angle in the lower mass ratio limit is consistent with the orientation shift of the most unstable linear tearing mode in an electron-scale current sheet.
C1 [Liu, Yi-Hsin; Hesse, M.; Kuznetsova, M.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Liu, YH (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM yhliu10@gmail.com
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NASA; MMS mission
FX Y. -H. Liu thanks W. Daughton, D. G. Sibeck, C. M. Komar, N. Bessho, J.
C. Dorelli, P. Cassak, N. Aunai, L. -J Chen, D. Wendel, M. L. Adrian, I.
Honkonen, and L. B. Wilson III for their helpful discussions. We are
grateful for the support from NASA through the NASA Postdoctoral Program
and MMS mission. Simulations were performed at the National Energy
Research Scientific Computing Center, NASA Advanced Supercomputing
Division and through LANL Institutional Computing Program. The
simulation data are available upon the request to the corresponding
author.
NR 57
TC 2
Z9 2
U1 4
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 SEP
PY 2015
VL 120
IS 9
BP 7331
EP 7341
DI 10.1002/2015JA021324
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800018
ER
PT J
AU Sundberg, T
Boardsen, SA
Burgess, D
Slavin, JA
AF Sundberg, Torbjoern
Boardsen, Scott A.
Burgess, David
Slavin, James A.
TI Coherent wave activity in Mercury's magnetosheath
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Mercury; magnetosheath; ion cyclotron waves
ID ION-CYCLOTRON WAVES; PLASMA DEPLETION LAYER; LOW-FREQUENCY WAVES;
MESSENGER OBSERVATIONS; BOW SHOCK; SOLAR-WIND; ANISOTROPY INSTABILITIES;
SUBSOLAR MAGNETOSHEATH; MAGNETIC-FIELD; UPSTREAM
AB This study presents a statistical overview of coherent wave activity in Mercury's magnetosheath. Left-handed electromagnetic ion cyclotron waves are commonly found behind the quasi-perpendicular section of the bow shock, where they are present in similar to 50% of the spacecraft crossings of the magnetosheath. Their occurrence distribution maximizes within the magnetosheath, approximately halfway between the bow shock and the magnetopause, and the waves are generally strongly Doppler shifted up to frequencies above the local ion cyclotron frequency. Downstream of the quasi-parallel shock, the magnetosheath often exhibits large-amplitude pulsations with wave periods around 10s and peak-to-peak amplitudes of up to 100nT that dominate the magnetic field structure. These waves are circularly left-hand polarized with wave vectors in the direction of the local shock normal. The data suggest that they have been generated upstream of the shock and transmitted into the downstream region. Their occurrence rates maximize at the near-parallel shock, where they are present approximately 10% of the time, and where they also show their largest wave powers. Some evidence is also found of waves with a right-handed polarization in the spacecraft frame. These consist of both whistler waves above the local ion cyclotron frequency and ion cyclotron waves propagating against the magnetosheath flow with Doppler shifts exceeding the intrinsic wave frequency, which results in a change in their apparent polarization. These waves are in minority compared to the left-handed observations, which indicates a preference for ion cyclotron waves propagating in the direction of the plasma flow.
C1 [Sundberg, Torbjoern; Burgess, David] Queen Mary Univ London, Sch Phys & Astron, London, England.
[Boardsen, Scott A.] Univ Maryland, Goddard Planetary Heliophys Inst, Baltimore, MD 21201 USA.
[Boardsen, Scott A.] NASA Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.
[Slavin, James A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Sundberg, T (reprint author), Queen Mary Univ London, Sch Phys & Astron, London, England.
EM t.sundberg@qmul.ac.uk
RI Slavin, James/H-3170-2012
OI Slavin, James/0000-0002-9206-724X
FU European Commission [284515]
FX We thank MESSENGER mission, the MESSENGER Magnetometer Instrument team,
and the Planetary Data System (https://pds.nasa.gov) for providing the
data used in this study. Parts of this work have been funded by the
European Commission's Seventh Framework Programme FP7 under the grant
agreement SHOCK (project number 284515).
NR 50
TC 1
Z9 1
U1 3
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2015
VL 120
IS 9
BP 7342
EP 7356
DI 10.1002/2015JA021499
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800019
ER
PT J
AU Macek, WM
Wawrzaszek, A
Sibeck, DG
AF Macek, W. M.
Wawrzaszek, A.
Sibeck, D. G.
TI THEMIS observation of intermittent turbulence behind the quasi-parallel
and quasi-perpendicular shocks
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE turbulence; intermittency; shocks; solar wind; magnetosheath; space
plasma
ID SOLAR-WIND TURBULENCE; MAGNETIC-FIELD; MAGNETOHYDRODYNAMIC TURBULENCE;
MULTIFRACTAL STRUCTURE; TERMINATION SHOCK; CASCADE MODEL; FLUCTUATIONS;
HELIOSHEATH; SPECTRUM; PLASMA
AB Turbulence is complex behavior that is ubiquitous in nature, but its mechanism is still not sufficiently clear. Therefore, the main aim of this paper is analysis of intermittent turbulence in magnetospheric and solar wind plasmas using a statistical approach based on experimental data acquired from space missions. The quintet spacecraft of Time History of Events and Macroscale Interactions during Substorms (THEMIS) allows us to investigate the details of turbulent plasma parameters behind the collisionless shocks. We investigate both the solar wind and magnetospheric data by using statistical probability distribution functions of Elsasser variables that can reveal the intermittent character of turbulence in space plasma. Our results suggest that turbulence behind the quasi-perpendicular shock is more intermittent with larger kurtosis than that behind the quasi-parallel shocks, which are immersed in a relatively quiet solar wind plasma, as confirmed by Wind measurements. It seems that behind the quasi-perpendicular shock the waves propagating outward from the Sun are larger than possibly damped waves propagating inward. In particular, we hope that this difference in characteristic behavior of the fluctuating space plasma parameters behind both types of shocks can help identify complex plasma structures in the future space missions. We also expect that the results obtained in this paper will be important for general models of turbulence.
C1 [Macek, W. M.] Cardinal Stefan Wyszy nski Univ, Fac Math & Nat Sci, Warsaw, Poland.
[Macek, W. M.; Wawrzaszek, A.] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland.
[Macek, W. M.; Sibeck, D. G.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Macek, WM (reprint author), Cardinal Stefan Wyszy nski Univ, Fac Math & Nat Sci, Warsaw, Poland.
EM macek@cbk.waw.pl
FU THEMIS project; European Community [313038/STORM]; National Science
Center, Poland (NCN) [2014/15/B/ST9/04782]
FX The research leading to these results has received funding from the
THEMIS project during a visit of W.M. at the NASA Goddard Space Flight
Center. This work has been supported by the European Community's Seventh
Framework Programme ([FP7/2007-2013]) under grant agreement 313038/STORM
and also by the National Science Center, Poland (NCN), through grant
2014/15/B/ST9/04782. We would like to thank the plasma and magnetic
field instruments team of THEMIS and Wind missions for providing the
data, which are available online from http://cdaweb.gsfc.nasa.gov.
NR 42
TC 2
Z9 2
U1 1
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2015
VL 120
IS 9
BP 7466
EP 7476
DI 10.1002/2015JA021656
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800027
ER
PT J
AU Birn, J
Hesse, M
Runov, A
Zhou, XZ
AF Birn, J.
Hesse, M.
Runov, A.
Zhou, X. -Z.
TI Ion beams in the plasma sheet boundary layer
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE ion beams; energetic ions; plasma sheet boundary layer; substorms
ID MAGNETIC RECONNECTION; SUBSTORM RECOVERY; AURORAL BULGE; DISTRIBUTIONS;
ELECTRON; MAGNETOTAIL; INJECTIONS; MAGNETOSPHERE; ENERGIZATION;
ACCELERATION
AB We explore characteristics of energetic particles in the plasma sheet boundary layer associated with dipolarization events, based on simulations and observations. The simulations use the electromagnetic fields of an MHD simulation of magnetotail reconnection and flow bursts as basis for test particle tracing. They are complemented by self-consistent fully electrodynamic particle-in-cell (PIC) simulations. The test particle simulations confirm that crescent-shaped earthward flowing ion velocity distributions with strong perpendicular anisotropy can be generated as a consequence of near-tail reconnection, associated with earthward flows and propagating magnetic field dipolarization fronts. Both PIC and test particle simulations show that the ion distribution in the outflow region close to the reconnection site also consist of a beam superposed on an undisturbed population, which, however, does not show strong perpendicular anisotropy. This suggests that the crescent shape is created by quasi-adiabatic deformation from ion motion along the magnetic field toward higher field strength. The simulation results compare favorably with Time History of Events and Macroscale Interactions during Substorms observations.
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 USA.
[Runov, A.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA.
[Zhou, X. -Z.] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China.
RP Birn, J (reprint author), Space Sci Inst, Boulder, CO 80301 USA.
EM jbirn@spacescience.org
RI Zhou, Xuzhi/D-1831-2011; NASA MMS, Science Team/J-5393-2013
OI Zhou, Xuzhi/0000-0003-4953-1761; NASA MMS, Science
Team/0000-0002-9504-5214
FU U.S. Department of Energy - NASA [NNX13AD10G, NNX13AD21G]; NSF
[1203711]; NASA [NAS5-0299, NNX13AF81G]; DLR contract [50 OC 0302]; ISSI
FX The simulation work was performed at Los Alamos under the auspices of
the U.S. Department of Energy, supported by NASA grants NNX13AD10G,
NNX13AD21G, and NSF grant 1203711. THEMIS data analysis was supported by
NASA grants NAS5-0299 and NNX13AF81G. We thank V. Angelopoulos for the
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, 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. This work also
grew out of a workshop on jet fronts at the International Space Science
Institute (ISSI), Bern, Switzerland, and we thank ISSI for its support.
Data necessary to understand, evaluate, replicate, and build upon the
reported research will be made available upon request.
NR 42
TC 2
Z9 2
U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2015
VL 120
IS 9
BP 7522
EP 7535
DI 10.1002/2015JA021573
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800031
ER
PT J
AU Remya, B
Tsurutani, BT
Reddy, RV
Lakhina, GS
Hajra, R
AF Remya, B.
Tsurutani, B. T.
Reddy, R. V.
Lakhina, G. S.
Hajra, R.
TI Electromagnetic cyclotron waves in the dayside subsolar outer
magnetosphere generated by enhanced solar wind pressure: EMIC wave
coherency
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE cyclotron waves; EMIC; wave coherency; pitch angle scattering
ID PITCH-ANGLE SCATTERING; INTERPLANETARY MAGNETIC-FIELD; RADIATION-BELT;
ELECTRON PRECIPITATION; PARTICLE INTERACTIONS; INTERACTION REGIONS;
GEOMAGNETIC STORMS; HIGH-INTENSITY; LONG-DURATION; CHORUS
AB Electromagnetic ion (proton) cyclotron (EMIC) waves and whistler mode chorus are simultaneously detected in the Earth's dayside subsolar outer magnetosphere. The observations were made near the magnetic equator 3.1 degrees-1.5 degrees magnetic latitude at 1300magnetic local time from L = 9.9 to 7.0. It is hypothesized that the solar wind external pressure caused preexisting energetic 10-100keV protons and electrons to be energized in the T component by betatron acceleration and the resultant temperature anisotropy (T>T-vertical bar) formed led to the simultaneous generation of both EMIC (ion) and chorus (electron) waves. The EMIC waves had maximum wave amplitudes of approximate to 6nT in a approximate to 60nT ambient field B-0. The observed EMIC wave amplitudes were about approximate to 10 times higher than the usually observed chorus amplitudes (approximate to 0.1-0.5nT). The EMIC waves are found to be coherent to quasi-coherent in nature. Calculations of relativistic approximate to 1-2MeV electron pitch angle transport are made using the measured wave amplitudes and wave packet lengths. Wave coherency was assumed. Calculations show that in a approximate to 25-50ms interaction with an EMIC wave packet, relativistic electron can be transported approximate to 27 degrees in pitch. Assuming dipole magnetic field lines for a L = 9 case, the cyclotron resonant interaction is terminated approximate to 20 degrees away from the magnetic equator due to lack of resonance at higher latitudes. It is concluded that relativistic electron anomalous cyclotron resonant interactions with coherent EMIC waves near the equatorial plane is an excellent loss mechanism for these particles. It is also shown that E > 1MeV electrons cyclotron resonating with coherent chorus is an unlikely mechanism for relativistic microbursts. Temporal structures of approximate to 30keV precipitating protons will be approximate to 2-3s which will be measurable at the top of the ionosphere.
C1 [Remya, B.; Reddy, R. V.; Lakhina, G. S.] Indian Inst Geomagnetism, Navi Mumbai, India.
[Remya, B.] Acad Sinica, Inst Earth Sci, Taipei 115, Taiwan.
[Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Hajra, R.] Inst Nacl Pesquisas Espaciais, BR-12201 Sao Jose Dos Campos, Brazil.
RP Remya, B (reprint author), Indian Inst Geomagnetism, Navi Mumbai, India.
EM remyaphysics@gmail.com
OI Remya, Bhanu/0000-0001-8356-8942; Lakhina, Gurbax /0000-0002-8956-486X;
Hajra, Rajkumar/0000-0003-0447-1531
FU Indian Institute of Geomagnetism, Navi Mumbai, India; NASA; National
Academy of Sciences, India (NASI)
FX B. Remya would like to thank Indian Institute of Geomagnetism, Navi
Mumbai, India, for providing her with Nanabhoy Moos Postdoctoral
Fellowship to carry out this research work. Portions of this research
were performed at the Jet Propulsion Laboratory, California Institute of
Technology under contract with NASA. G.S.L. thanks the National Academy
of Sciences, India (NASI) for the support under the NASI-Senior
Scientist Platinum Jubilee Fellowship. The solar wind and interplanetary
magnetic field data are obtained from the OMNI website
(http://omniweb.gsfc.nasa.gov/). One minute AE indices and 1 h SYM-H
indices were obtained from the World Data Center for Geomagnetism,
Kyoto, Japan (http://wdc.kugi.kyoto-u.ac.jp/). The integrated fluxes of
electrons with energies E > 2.0 MeV are obtained from GOES-8
(http://www.ngdc.noaa.gov/stp/satellite/goes/dataaccess.html). The
Cassini fluxgate magnetometer data are obtained from NASA Planetary Data
System (http://ppi.pds.nasa.gov/).
NR 79
TC 5
Z9 5
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 SEP
PY 2015
VL 120
IS 9
BP 7536
EP 7551
DI 10.1002/2015JA021327
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800032
ER
PT J
AU Adrian, ML
Fung, SF
Gallagher, DL
Green, JL
AF Adrian, M. L.
Fung, S. F.
Gallagher, D. L.
Green, J. L.
TI Whistlers observed outside the plasmasphere: Correlation to
plasmaspheric/plasmapause features
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE plasmasphere; plasma waves and instabilities; magnetosphere-ionosphere
coupling; plasma convection
ID EXTREME-ULTRAVIOLET IMAGER; PERIODIC VLF EMISSIONS; FIELD-ALIGNED
COLUMNS; EARTHS MAGNETOSPHERE; ENHANCED IONIZATION; MAGNETIC EQUATOR;
MODE WAVES; PROPAGATION; PLASMAPAUSE; DENSITY
AB Whistlers observed outside the plasmasphere by Cluster have been correlated with the global plasmasphere using Imager for Magnetopause-to-Aurora Global Exploration-Extreme Ultraviolet Imager (IMAGE-EUV) observations. Of the 12 Cluster-observed whistler events reported, EUV is able to provide global imaging of the plasmasphere for every event and demonstrates a direct correlation between the detection of lightning-generated whistlers beyond the plasmapause and the presence of a global perturbation of the local plasmapause. Of these 12 correlated events, seven of the Cluster-observed whistlers (or 58%) are associated with the Cluster spacecraft lying radially outward from a plasmaspheric notch. Two of the Cluster-observed whistlers (17%) are associated with the low-density region between the late afternoon plasmapause and the western wall of a plasmaspheric drainage plume. The final three Cluster-observed whistler events (25%) are associated with a nonradial, nonazimuthal depletion in plasmaspheric He+ emission that are termed notch-like crenulations. In one of these cases, the notch-like crenulations appear to be manifestations entrained within the plasmasphere boundary layer of a standing wave on the surface of the plasmasphere. The correlated Cluster/IMAGE-EUV observations suggest that the depleted flux tubes that connect the ionosphere to the low-density regions of plasmaspheric trough and inner magnetosphere facilitate the escape of whistler waves from the plasmasphere.
C1 [Adrian, M. L.; Fung, S. F.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gallagher, D. L.] NASA Marshall Space Flight Ctr, Huntsville, AL USA.
[Green, J. L.] NASA Headquarters, Washington, DC USA.
RP Adrian, ML (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Mark.L.Adrian@nasa.gov
FU IMAGE mission through the NASA Office of Space Science
FX The IMAGE mission through the NASA Office of Space Science has supported
this research. The authors would like to thank Michelle Thomson for
providing the LANL-MPA data presented herein. In addition, the authors
thank Jolene Pickett for numerous discussions concerning the use of
Cluster Wide Band data that formed the basis of this effort. Also, we
would like to thank the Cluster-WHISPER instrument team and the Cluster
Science Archive for providing data used in this study. IMAGE-EUV data,
analysis tools, and quick-look movie products are publicly available
through the IMAGE Extreme Ultraviolet Imager website, Lunar and
Planetary Laboratory, University of Arizona
(http://euv.lpl.arizona.edu/euv/). Cluster WBD and WHISPER data are
available, via registration, through the Cluster Science Archive
(http://www.cosmos.esa.int/web/csa/access). Public access to LANL-MPA
quick-look data products is through the Los Alamos National Laboratory,
Los Alamos Magnetospheric Plasma Analyzer (MPA) website
(http://www.mpa.lanl.gov/index.shtml).
NR 61
TC 0
Z9 0
U1 3
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2015
VL 120
IS 9
BP 7585
EP 7614
DI 10.1002/2014JA020811
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800034
ER
PT J
AU Kanekal, SG
Baker, DN
Henderson, MG
Li, W
Fennell, JF
Zheng, Y
Richardson, IG
Jones, A
Ali, AF
Elkington, SR
Jaynes, A
Li, X
Blake, JB
Reeves, GD
Spence, HE
Kletzing, CA
AF Kanekal, S. G.
Baker, D. N.
Henderson, M. G.
Li, W.
Fennell, J. F.
Zheng, Y.
Richardson, I. G.
Jones, A.
Ali, A. F.
Elkington, S. R.
Jaynes, A.
Li, X.
Blake, J. B.
Reeves, G. D.
Spence, H. E.
Kletzing, C. A.
TI Relativistic electron response to the combined magnetospheric impact of
a coronal mass ejection overlapping with a high-speed stream: Van Allen
Probes observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE relativistic electrons; IP shock; CME; HSS
ID RADIATION-BELT ELECTRONS; GEOMAGNETIC STORMS; ENERGETIC PARTICLE;
ACCELERATION; EVENTS; TIME; DIFFUSION; SAMPEX; CHORUS; INNER
AB During early November 2013, the magnetosphere experienced concurrent driving by a coronal mass ejection (CME) during an ongoing high-speed stream (HSS) event. The relativistic electron response to these two kinds of drivers, i.e., HSS and CME, is typically different, with the former often leading to a slower buildup of electrons at larger radial distances, while the latter energizing electrons rapidly with flux enhancements occurring closer to the Earth. We present a detailed analysis of the relativistic electron response including radial profiles of phase space density as observed by both Magnetic Electron and Ion Sensor (MagEIS) and Relativistic Electron Proton Telescope instruments on the Van Allen Probes mission. Data from the MagEIS instrument establish the behavior of lower energy (<1MeV) electrons which span both intermediary and seed populations during electron energization. Measurements characterizing the plasma waves and magnetospheric electric and magnetic fields during this period are obtained by the Electric and Magnetic Field Instrument Suite and Integrated Science instrument on board Van Allen Probes, Search Coil Magnetometer and Flux Gate Magnetometer instruments on board Time History of Events and Macroscale Interactions during Substorms, and the low-altitude Polar-orbiting Operational Environmental Satellites. These observations suggest that during this time period, both radial transport and local in situ processes are involved in the energization of electrons. The energization attributable to radial diffusion is most clearly evident for the lower energy (<1MeV) electrons, while the effects of in situ energization by interaction of chorus waves are prominent in the higher-energy electrons.
C1 [Kanekal, S. G.; Zheng, Y.; Richardson, I. G.; Jones, A.; Li, X.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Baker, D. N.; Ali, A. F.; Elkington, S. R.; Jaynes, A.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Henderson, M. G.; Reeves, G. D.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Li, W.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Blake, J. B.] Aerosp Corp, Los Angeles, CA 90009 USA.
[Richardson, I. G.] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA.
[Jones, A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Kletzing, C. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
RP Kanekal, SG (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM shrikanth.g.kanekal@nasa.gov
RI Reeves, Geoffrey/E-8101-2011; Henderson, Michael/A-3948-2011;
OI Reeves, Geoffrey/0000-0002-7985-8098; Henderson,
Michael/0000-0003-4975-9029; Kletzing, Craig/0000-0002-4136-3348;
Richardson, Ian/0000-0002-3855-3634; Ali, Ashar/0000-0003-2981-5791
FU JHU/APL contract under NASA's prime contract [967399, NAS5-01072];
EMFISIS subaward [1001057397:01]; ECT subaward [13-041]; NASA
[NNX11AD75G, NNX11AR64G, NNX13AI61G, NNX15AF61G]; NSF [AGS 1405054]
FX The work at LASP, University of Colorado supported by JHU/APL contract
967399 under NASA's prime contract NAS5-01072. the work at UCLA was
supported by the EMFISIS subaward 1001057397:01, ECT subaward 13-041,
NASA grants NNX11AD75G, NNX11AR64G, NNX13AI61G, and NNX15AF61G, and the
NSF grant AGS 1405054. All the MagEIS and REPT, Van Allen Probes data
used are publicly available at (www.rbsp-ect.lanl.gov).
NR 51
TC 4
Z9 4
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 SEP
PY 2015
VL 120
IS 9
BP 7629
EP 7641
DI 10.1002/2015JA021395
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800036
ER
PT J
AU Gutynska, O
Sibeck, DG
Omidi, N
AF Gutynska, O.
Sibeck, D. G.
Omidi, N.
TI Magnetosheath plasma structures and their relation to foreshock
processes
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE magnetosheath; plasma structures; foreshock
ID DYNAMIC PRESSURE VARIATIONS; LOW-FREQUENCY VARIATIONS; SOLAR-WIND;
MAGNETIC-FIELD; DENSITY-FLUCTUATIONS; EARTHS MAGNETOSHEATH;
QUASI-PARALLEL; SPACECRAFT; FEATURES; FLUX
AB We present simultaneous Time History of Events and Macroscale Interactions during Substorms observations of plasma parameters upstream in the solar wind and downstream in the magnetosheath (MSH) from 2007 to 2008. We discuss the connection of foreshock (FSH) processes and magnetospheric disturbances to transmission mechanisms in the MSH. In 60% of the analyzed cases, the MSH was strongly influenced by the FSH. We analyze the results as a function of location, time scale, spatial orientation of the observed structures, and the prevailing interplanetary magnetic field (IMF) and solar wind plasma parameters. We find that plasma structures with density enhancement are mostly observed during radial IMF orientations and for small (BN), the angle between the upstream magnetic field and the local bow shock normal; the observed structures are pressure balanced with strong anticorrelation between density and temperature; the scale size of the density fluctuations is about 0.4R(E). We compare the observations with results from a 2.5-dimensional hybrid simulation to investigate the mechanisms by which the foreshock plasma structures are generated, propagate through the bow shock, and evolve.
C1 [Gutynska, O.; Sibeck, D. G.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Omidi, N.] Solana Sci Inc, Solana Beach, CA USA.
RP Gutynska, O (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM olga.gutynska@nasa.gov
FU NASA; NASA's THEMIS project; NSF [AGS-1007449]
FX This research was supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. The work of D.
Sibeck was supported by NASA's THEMIS project. N. Omidi acknowledges
support by NSF grant AGS-1007449. We thank the NASA CDAWeb for providing
data. Simulation results have been provided by N. Omidi and are
available upon request (omidi@solanasci.com).
NR 32
TC 3
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U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2015
VL 120
IS 9
BP 7687
EP 7697
DI 10.1002/2014JA020880
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800040
ER
PT J
AU Birn, J
Runov, A
Hesse, M
AF Birn, J.
Runov, A.
Hesse, M.
TI Energetic ions in dipolarization events
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE ion acceleration; dipolarization events
ID TEST PARTICLE ORBITS; GEOSYNCHRONOUS OBSERVATIONS; FLUX BUNDLES;
ELECTRONS; SUBSTORMS; ACCELERATION; MAGNETOTAIL; TRANSPORT; PLASMA;
ENERGIZATION
AB We investigate ion acceleration in dipolarization events in the magnetotail, using the electromagnetic fields of an MHD simulation of magnetotail reconnection and flow bursts as basis for test particle tracing. The simulation results are compared with Time History of Events and Macroscale Interactions during Substorms observations. We provide quantitative answers to the relative importance of source regions and source energies. Flux decreases at proton energies up to 10-20keV are found to be due to sources of lobe or plasma sheet boundary layer particles that enter the near tail via reconnection. Flux increases result from both thermal and suprathermal ion sources. Comparable numbers of accelerated protons enter the acceleration region via cross-tail drift from the dawn flanks of the near-tail plasma sheet and via reconnection of field lines extending into the more distant tail. We also demonstrate the presence of earthward plasma flow and accelerated suprathermal ions ahead of a dipolarization front. The flow acceleration stems from a net Lorentz force, resulting from reduced pressure gradients within a pressure pile-up region ahead of the front. Suprathermal precursor ions result from, typically multiple reflections at the front. Low-energy ions also become accelerated due to inertial drift in the direction of the small precursor electric field.
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 by NASA [NNX13AD10G, NNX14AI18G]; NSF
[1203711]; NASA [NAS5-0299, NNX13AF81G]; DLR [50 OC 0302]; International
Space Science Institute, Bern, Switzerland
FX The simulation work was performed at Los Alamos National Laboratory
under the auspices of the U.S. Department of Energy, supported by NASA
grants NNX13AD10G and NNX14AI18G, and NSF grant 1203711. THEMIS data
analysis was supported by NASA grants NAS5-0299 and NNX13AF81G. We thank
V. Angelopoulos for the use of data from the THEMIS Mission, C.W.
Carlson and J.P. McFadden for use of ESA data, D. Larson, R.P. Lin for
use of SST data, D.L. Turner and P. Cruce for help with SST data
calibration, 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 for the hospitality and support by the
International Space Science Institute, Bern, Switzerland, and the
fruitful discussions with members of the ISSI working group. Data
necessary to understand, evaluate, replicate, and build upon the
reported research will be made available upon request.
NR 53
TC 5
Z9 5
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2015
VL 120
IS 9
BP 7698
EP 7717
DI 10.1002/2015JA021372
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800041
ER
PT J
AU Doss, CE
Komar, CM
Cassak, PA
Wilder, FD
Eriksson, S
Drake, JF
AF Doss, C. E.
Komar, C. M.
Cassak, P. A.
Wilder, F. D.
Eriksson, S.
Drake, J. F.
TI Asymmetric magnetic reconnection with a flow shear and applications to
the magnetopause
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE magnetic reconnection; flow shear; polar cusps; magnetopause; asymmetric
ID HIGH-LATITUDE MAGNETOPAUSE; SOLAR-WIND INTERACTION; NORTHWARD IMF;
PLASMASPHERIC PLUME; COLLISIONLESS RECONNECTION; DAYSIDE MAGNETOPAUSE;
TEARING INSTABILITY; EARTHS MAGNETOPAUSE; TAIL MAGNETOPAUSE; PLASMA-FLOW
AB We perform a systematic theoretical and numerical study of antiparallel two-dimensional magnetic reconnection with asymmetries in the plasma density and reconnecting magnetic field strength in addition to a bulk flow shear across the reconnection site in the plane of the reconnecting fields, which commonly occurs at planetary magnetospheres. We analytically predict the speed at which an isolated X line is convected by the flow, the reconnection rate, and the critical flow speed at which reconnection no longer takes place for arbitrary reconnecting magnetic field strengths, densities, and upstream flow speeds, and we confirm the results with two-fluid numerical simulations. The predictions and simulation results counter the prevailing model of reconnection at Earth's dayside magnetopause which says reconnection occurs with a stationary X line for sub-Alfvenic magnetosheath flow, reconnection occurs but the X line convects for magnetosheath flows between the Alfven speed and double the Alfven speed, and reconnection does not occur for magnetosheath flows greater than double the Alfven speed. In particular, we find that X line motion is governed by momentum conservation from the upstream flows, which are weighted differently in asymmetric systems, so the X line convects for generic conditions including sub-Alfvenic upstream speeds. For the reconnection rate, as with symmetric reconnection, it drops with increasing flow shear and there is a cutoff speed above which reconnection is not predominant. However, while the cutoff condition for symmetric reconnection is that the difference in flows on the two sides of the reconnection site is twice the Alfven speed, we find asymmetries cause the cutoff speed for asymmetric reconnection to be higher than twice the asymmetric form of the Alfven speed. The stronger the asymmetries, the more the cutoff exceeds double the asymmetric Alfven speed. This is due to the fact that in asymmetric reconnection, the plasma with the smaller mass flux into the dissipation region contributes a smaller mass to the dissipation region, so the effect of its flow on opposing the release of energy by the reconnected magnetic fields is diminished and the reconnection is not suppressed to the extent previously thought. The results compare favorably with an observation of reconnection at Earth's polar cusps during a period of northward interplanetary magnetic field, where reconnection occurs despite the magnetosheath flow speed being more than twice the magnetosheath Alfven speed, the previously proposed suppression condition. These results are expected to be of broad importance for magnetospheric physics of Earth and other planets; particular applications are discussed.
C1 [Doss, C. E.; Komar, C. M.; Cassak, P. A.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
[Komar, C. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wilder, F. D.; Eriksson, S.] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO USA.
[Drake, J. F.] Univ Maryland, Inst Res Electrons & Appl Phys, College Pk, MD 20742 USA.
RP Cassak, PA (reprint author), W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
EM Paul.Cassak@mail.wvu.edu
OI Komar, Colin/0000-0001-5850-7507; Eriksson, Stefan/0000-0002-5619-1577
FU NASA West Virginia Space Grant Consortium; West Virginia University
Summer Undergraduate Research Experience (SURE) program; NSF
[AGS-0953463]; International Space Science Institute in Bern,
Switzerland; Office of Science of the U.S. Department of Energy
[DE-AC02-05CH11231]
FX Support from NASA West Virginia Space Grant Consortium (C.E.D. and
C.M.K.), the West Virginia University Summer Undergraduate Research
Experience (SURE) program (C.E.D.), and NSF Grant AGS-0953463 (P.A.C.)
is gratefully acknowledged. P.A.C. acknowledges support from the
International Space Science Institute in Bern, Switzerland. This
research used resources of the National Energy Research Scientific
Computing Center, a DOE Office of Science User Facility supported by the
Office of Science of the U.S. Department of Energy under Contract No.
DE-AC02-05CH11231. The data used to produce the results of this paper
are available from the authors. We thank M. T. Beidler, R. C. Fear, S.
A. Fuselier, and B. M. Walsh for helpful conversations.
NR 87
TC 7
Z9 7
U1 0
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 SEP
PY 2015
VL 120
IS 9
BP 7748
EP 7763
DI 10.1002/2015JA021489
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800045
ER
PT J
AU Fytterer, T
Santee, ML
Sinnhuber, M
Wang, S
AF Fytterer, T.
Santee, M. L.
Sinnhuber, M.
Wang, S.
TI The 27day solar rotational effect on mesospheric nighttime OH and O-3
observations induced by geomagnetic activity
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE 27day solar rotational signal; geomagnetic activity; ozone; mesosphere
ID MICROWAVE LIMB SOUNDER; EVENTS; ATMOSPHERE; JANUARY; OZONE; CYCLE
AB Observations performed by the Earth Observing System Microwave Limb Sounder instrument on board the Aura satellite from 2004 to 2009 (2004 to 2014) were used to investigate the 27day solar rotational cycle in mesospheric OH (O-3) and the physical connection to geomagnetic activity. Data analysis was focused on nighttime measurements at geomagnetic latitudes connected to the outer radiation belts (55 degrees N/S-75 degrees N/S). The applied superposed epoch analysis reveals a distinct 27day solar rotational signal in OH and O-3 during winter in both hemispheres at altitudes >70km. The OH response is positive and in-phase with the respective geomagnetic activity signal, lasting for 1-2days. In contrast, the O-3 feedback is negative, delayed by 1day, and is present up to 4days afterward. Largest OH (O-3) peaks are found at similar to 75km, exceeding the 95% significance level and the measurement noise of <2% (<0.5%), while reaching variations of +14% (-7%) with respect to their corresponding background. OH at 75km is observed to respond to particle precipitation only after a certain threshold of geomagnetic activity is exceeded, depending on the respective OH background. The relation between OH and O-3 at 75km in both hemispheres is found to be nonlinear. In particular, OH has a strong impact on O-3 for relatively weak geomagnetic disturbances and accompanying small absolute OH variations (<0.04ppb). In contrast, catalytic O-3 depletion is seen to slow down for stronger geomagnetic variations and OH anomalies (0.04-0.13ppb), revealing small variations around -0.11ppm.
C1 [Fytterer, T.; Sinnhuber, M.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, Eggenstein Leopoldshafen, Germany.
[Santee, M. L.; Wang, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Fytterer, T (reprint author), Karlsruhe Inst Technol, Inst Meteorol & Climate Res, Eggenstein Leopoldshafen, Germany.
EM tilo.fytterer@kit.edu
FU NASA; Helmholtz Association of German Research Centres (HGF)
[VH-NG-624]; Deutsche Forschungsgemeinschaft; Open Access Publishing
Fund of Karlsruhe Institute of Technology
FX The data used in this study are completely freely accessible to the
public and were downloaded from http://mls.jpl.nasa.gov/ (level 2 OH and
O3 measurements, version 3.3/3.4),
http://www.ngdc.noaa.gov/geomag/data/poles/NP. xy (Earth's magnetic
North Pole coordinates), http://umbra.nascom.nasa.gov/SEP/ (date of
solar proton events),
ftp://ftp.ngdc.noaa.gov/STP/GEOMAGNETIC_DATA/INDICES/KP_AP/ (daily Ap
index values), and http://lasp.colorado.edu/lisird/lya/ (daily Lyman
alpha values). Work at the Jet Propulsion Laboratory, California
Institute of Technology, was done under contract with NASA. T. Fytterer
and M. Sinnhuber gratefully acknowledge funding by the Helmholtz
Association of German Research Centres (HGF), grant VH-NG-624. The
authors further acknowledge support by Deutsche Forschungsgemeinschaft
and Open Access Publishing Fund of Karlsruhe Institute of Technology.
NR 21
TC 4
Z9 4
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2015
VL 120
IS 9
BP 7926
EP 7936
DI 10.1002/2015JA021183
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800057
PM 27774372
ER
PT J
AU Verkhoglyadova, OP
Mannucci, AJ
Ao, CO
Iijima, BA
Kursinski, ER
AF Verkhoglyadova, O. P.
Mannucci, A. J.
Ao, C. O.
Iijima, B. A.
Kursinski, E. R.
TI Effect of small-scale ionospheric variability on GNSS radio occultation
data quality
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE ionosphere; atmospheric refractivity; radio occultations
ID SPORADIC-E LAYER; MORPHOLOGY; PROFILES; SIGNALS
AB Global Navigation Satellite Systems (GNSS) radio occultation (RO) measurements are sensitive to thin ionization layers and small-scale ionosphere structures. To evaluate error bounds and possible biases in atmospheric retrievals, we characterized ionospheric irregularities encountered in the affected profiles by analyzing the L1 signal-to-noise ratio (SNR) variability at E layer altitudes (from 90km to 130km). New metrics to analyze statistical effects of small-scale ionospheric irregularities on refractivity retrievals are proposed. We analyzed refractivity (N) retrievals with Constellation Observing System for Meteorology, Ionosphere and Climate (COSMIC) ROs in 2011. Using refractivity from European Centre for Medium-Range Weather Forecasts (ECMWF) analysis (N-ECMWF) as the reference data set, we studied statistical properties of the fractional refractivity bias (N) defined by the difference (N-ECMWF-N)/N-ECMWF and averaged in the altitude range from 20 to 25km for each individual profile. We found that (1) persistently larger variability of the L1 SNR as measured by the interquartile range (IQR) existed when the occultation tangent point was in the 90km to 110km altitude range than at higher E layer altitudes; (2) the upper limits on the fractional refractivity bias for COSMIC ROs are 0.06% (for daytime local time), 0.1% (for nighttime local time), and similar to 0.01% (for all local times); (3) distributions of N are non-Gaussian (leptokurtic); (4) latitudinal distributions of small and large N for different levels of ionospheric variability show large tails (N-ECMWF>N) occurring around the Himalaya and the Andes regions, which are possibly due to biases in ECMWF analysis. We conclude that the refractivity bias due to small-scale irregularities is small below 25km altitude and can be neglected.
C1 [Verkhoglyadova, O. P.; Mannucci, A. J.; Ao, C. O.; Iijima, B. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Kursinski, E. R.] Moog Adv Miss & Sci, Golden, CO USA.
RP Verkhoglyadova, OP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Olga.Verkhoglyadova@jpl.nasa.gov
OI Verkhoglyadova, Olga/0000-0002-9295-9539
FU NASA
FX The work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the NASA. O.P.V. would
like to thank Panagiotis Vergados and Lawrence Young (JPL) for useful
discussions. ECMWF TOGA analysis data were provided by NOAA through
http://rda.ucar.edu/datasets/ds111.2/, COSMIC RO retrievals are
processed at the Jet Propulsion Laboratory,
http://genesis.jpl.nasa.gov/genesis/.
NR 32
TC 0
Z9 0
U1 5
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 SEP
PY 2015
VL 120
IS 9
BP 7937
EP 7951
DI 10.1002/2015JA021055
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800058
ER
PT J
AU Samara, M
Michell, RG
Redmon, RJ
AF Samara, M.
Michell, R. G.
Redmon, R. J.
TI Low-altitude satellite measurements of pulsating auroral electrons
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE precipitating electrons; secondary electrons; pulsating aurora; DMSP;
Reimei
ID PRECIPITATING ELECTRONS; MAGNETOSPHERE; IONOSPHERE
AB We present observations from the Defense Meteorological Satellite Program and Reimei satellites, where common-volume high-resolution ground-based auroral imaging data are available. These satellite overpasses of ground-based all-sky imagers reveal the specific features of the electron populations responsible for different types of pulsating aurora modulations. The energies causing the pulsating aurora mostly range from 3keV to 20keV but can at times extend up to 30keV. The secondary, low-energy electrons (<1keV) are diminished from the precipitating distribution when there are strong temporal variations in auroral intensity. There are often persistent spatial structures present inside regions of pulsating aurora, and in these regions there are secondary electrons in the precipitating populations. The reduction of secondary electrons is consistent with the strongly temporally varying pulsating aurora being associated with field-aligned currents and hence parallel potential drops of up to 1kV.
C1 [Samara, M.; Michell, R. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Michell, R. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Redmon, R. J.] NOAA, Boulder, CO USA.
RP Samara, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM marilia.samara@nasa.gov
FU NASA [NNX12AE76G, NNX13AG07G]; National Science Foundation [AGS-1456161,
AGS-1456129]
FX The authors thank Don Hampton for the assistance with imager setup and
operation at Poker Flat; SRI, specifically Eggert Gudmundsson and the
rest of the Sondrestrom crew for their assistance and hospitality; and
Mike Kosch for graciously allowing us the use of his imager enclosure in
Tromsoand JHU/APL for providing the DMSP precipitating electron
measurements. The authors are grateful to Masafumi Hirahara of STEL,
Nagoya University; Kazushi Asamura of ISAS/JAXA; and the Reimei team for
making their particle data and software easily accessible. DMSP, MOOSE,
and Reimei data are freely available. DMSP data can be obtained through
http://sd-www.jhuapl.edu/Aurora/spectrogram/index.html using the java
tool available for download. Reimei data and software can be obtained
through http://reimei.stelab.nagoya-u.ac.jp. MOOSE data can be obtained
through Marilia Samara, marilia.samara@nasa.gov. M.S. was supported by
NASA grant NNX12AE76G. R.M. was supported by National Science Foundation
grants AGS-1456161 and AGS-1456129. R.R. is a NOAA civil servant and was
partially funded by NASA grant NNX13AG07G.
NR 29
TC 1
Z9 1
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2015
VL 120
IS 9
BP 8111
EP 8124
DI 10.1002/2015JA021292
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU9PN
UT WOS:000363876800069
ER
PT J
AU Ramsey, E
Rangoonwala, A
Jones, CE
AF Ramsey, Elijah, III
Rangoonwala, Amina
Jones, Cathleen E.
TI Structural Classification of Marshes with Polarimetric SAR Highlighting
the Temporal Mapping of Marshes Exposed to Oil
SO REMOTE SENSING
LA English
DT Article
DE polarimetric radar; marsh structure mapping; LAI; LAD; UAVSAR; Deepwater
Horizon oil spill
ID LEAF-AREA INDEX; SCATTERING MODEL; FRESH-WATER; L-BAND; REFLECTANCE;
RADAR; VEGETATION; CANOPY; LOUISIANA; DECOMPOSITION
AB Empirical relationships between field-derived Leaf Area Index (LAI) and Leaf Angle Distribution (LAD) and polarimetric synthetic aperture radar (PolSAR) based biophysical indicators were created and applied to map S. alterniflora marsh canopy structure. PolSAR and field data were collected near concurrently in the summers of 2010, 2011, and 2012 in coastal marshes, and PolSAR data alone were acquired in 2009. Regression analyses showed that LAI correspondence with the PolSAR biophysical indicator variables equaled or exceeded those of vegetation water content (VWC) correspondences. In the final six regressor model, the ratio HV/VV explained 49% of the total 77% explained LAI variance, and the HH-VV coherence and phase information accounted for the remainder. HV/HH dominated the two regressor LAD relationship, and spatial heterogeneity and backscatter mechanism followed by coherence information dominated the final three regressor model that explained 74% of the LAD variance. Regression results applied to 2009 through 2012 PolSAR images showed substantial changes in marsh LAI and LAD. Although the direct cause was not substantiated, following a release of freshwater in response to the 2010 Deepwater Horizon oil spill, the fairly uniform interior marsh structure of 2009 was more vertical and dense shortly after the oil spill cessation. After 2010, marsh structure generally progressed back toward the 2009 uniformity; however, the trend was more disjointed in oil impact marshes.
C1 [Ramsey, Elijah, III; Rangoonwala, Amina] US Geol Survey, Natl Wetlands Res Ctr, Lafayette, LA 70506 USA.
[Jones, Cathleen E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ramsey, E (reprint author), US Geol Survey, Natl Wetlands Res Ctr, 700 Cajundome Blvd, Lafayette, LA 70506 USA.
EM ramseye@usgs.gov; rangoonwalaa@usgs.gov; cathleen.e.jones@jpl.nasa.gov
FU National Aeronautics Space Administration (NASA) [11-TE11-104]; NASA;
U.S. Geological Survey Hurricane Sandy Supplemental Funds
FX We thank Francis Fields Jr. of the Apache Louisiana Minerals LLC, a
subsidiary of Apache Corporation, for access to their properties, and
Jeff Deblieux IV of the Louisiana Land and Exploration Company, a
subsidiary of Conoco Phillips, for access to their properties. We are
indebted to late Clint Jeske and Steve Hartley of the U.S. Geological
Survey for their critical assistance in sample collections, Kevin Jones
and PCI Geomatics staff for timely solutions to complex image processing
obstacles, and Professor Yong Wang at East Caroline University for his
insightful and constructive review. Research was supported in part by
the National Aeronautics Space Administration (NASA) Grant #11-TE11-104
and was carried out in collaboration with the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA, and
supported in part by U.S. Geological Survey Hurricane Sandy Supplemental
Funds. UAVSAR data are provided courtesy of NASA/JPL-Caltech. Any use of
trade, firm, or product names is for descriptive purposes only and does
not imply endorsement by the U.S. Government.
NR 83
TC 2
Z9 2
U1 3
U2 12
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD SEP
PY 2015
VL 7
IS 9
BP 11295
EP 11321
DI 10.3390/rs70911295
PG 27
WC Remote Sensing
SC Remote Sensing
GA CT0UA
UT WOS:000362511400014
ER
PT J
AU Claverie, M
Vermote, E
Franch, B
He, T
Hagolle, O
Kadiri, M
Masek, J
AF Claverie, Martin
Vermote, Eric
Franch, Belen
He, Tao
Hagolle, Olivier
Kadiri, Mohamed
Masek, Jeff
TI Evaluation of Medium Spatial Resolution BRDF-Adjustment Techniques Using
Multi-Angular SPOT4 (Take5) Acquisitions
SO REMOTE SENSING
LA English
DT Article
DE surface anisotropy; BRDF; SPOT4 (Take5); MODIS
ID BIDIRECTIONAL REFLECTANCE; DIRECTIONAL SIGNATURES; SURFACE REFLECTANCE;
LANDSAT DATA; TIME-SERIES; MODIS DATA; IN-SITU; ALBEDO; RETRIEVAL;
VALIDATION
AB High-resolution sensor Surface Reflectance (SR) data are affected by surface anisotropy but are difficult to adjust because of the low temporal frequency of the acquisitions and the low angular sampling. This paper evaluates five high spatial resolution Bidirectional Reflectance Distribution Function (BRDF) adjustment techniques. The evaluation is based on the noise level of the SR Time Series (TS) corrected to a normalized geometry (nadir view, 45 degrees sun zenith angle) extracted from the multi-angular acquisitions of SPOT4 over three study areas (one in Arizona, two in France) during the five-month SPOT4 (Take5) experiment. Two uniform techniques (Cst, for Constant, and Av, for Average), relying on the Vermote-Justice-Breon (VJB) BRDF method, assume no variation in space of the BRDF shape. Two methods (VI-dis, for NDVI-based disaggregation and LC-dis, for Land-Cover based disaggregation) are based on disaggregation of the MODIS-derived BRDF VJB parameters using vegetation index and land cover, respectively. The last technique (LUM, for Look-Up Map) relies on the MCD43 MODIS BRDF products and a crop type data layer. The VI-dis technique produced the lowest level of noise corresponding to the most effective adjustment: reduction from directional to normalized SR TS noises by 40% and 50% on average, for red and near-infrared bands, respectively. The uniform techniques displayed very good results, suggesting that a simple and uniform BRDF-shape assumption is good enough to adjust the BRDF in such geometric configuration (the view zenith angle varies from nadir to 25 degrees). The most complex techniques relying on land cover (LC-dis and LUM) displayed contrasting results depending on the land cover.
C1 [Claverie, Martin; Franch, Belen; He, Tao] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Claverie, Martin; Vermote, Eric; Franch, Belen; Masek, Jeff] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hagolle, Olivier; Kadiri, Mohamed] Unite Mixte CNES CNRS IRD UPS, CESBIO, F-31401 Toulouse 4, France.
RP Claverie, M (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
EM martin.claverie@nasa.gov; eric.f.vermote@nasa.gov; befranch@umd.edu;
the@umd.edu; olivier.arino@esa.int; mohamed.kadiri@cesbio.cnes.fr;
jeffrey.g.masek@nasa.gov
RI Masek, Jeffrey/D-7673-2012; He, Tao/H-5130-2012
OI He, Tao/0000-0003-2079-7988
NR 35
TC 3
Z9 3
U1 3
U2 5
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD SEP
PY 2015
VL 7
IS 9
BP 12057
EP 12075
DI 10.3390/rs70912057
PG 19
WC Remote Sensing
SC Remote Sensing
GA CT0UA
UT WOS:000362511400051
ER
PT J
AU Hagolle, O
Sylvander, S
Huc, M
Claverie, M
Clesse, D
Dechoz, C
Lonjou, V
Poulain, V
AF Hagolle, Olivier
Sylvander, Sylvia
Huc, Mireille
Claverie, Martin
Clesse, Dominique
Dechoz, Cecile
Lonjou, Vincent
Poulain, Vincent
TI SPOT-4 (Take 5): Simulation of Sentinel-2 Time Series on 45 Large Sites
SO REMOTE SENSING
LA English
DT Article
DE Sentinel-2; SPOT-4 (Take 5); time series; repetitivity; image
registration; cloud detection; atmospheric correction; surface
reflectance; validation
ID IMAGERY; FORMOSAT-2; PRODUCTS; MISSION; LANDSAT; SURFACE
AB This paper presents the SPOT-4 (Take 5) experiment, aimed at providing time series of optical images simulating the repetitivity, the resolution and the large swath of Sentinel-2 images. The aim was to help users set up and test their applications and methods, before Sentinel-2 mission data become available. In 2016, when both Sentinel-2 satellites are operational, and for at least fifteen years, users will have access to high resolution time series of images systematically acquired every five days, over the whole Earth land surfaces. Thanks to Sentinel-2's high revisit frequency, a given surface should be observed without clouds at least once a month, except in the most cloudy periods and regions. In 2013, the Centre National d'Etudes Spatiales (CNES) lowered the orbit altitude of SPOT-4, to place it on a five-day repeat cycle orbit for a duration of five months. This experiment started on 31 January 2013 and lasted until 19 June 2013. SPOT-4 images were acquired every fifth day, over 45 sites scattered in nearly all continents and covering very diverse biomes for various applications. Two ortho-rectified products were delivered for each acquired image that was not fully cloudy, expressed either as top of atmosphere reflectance (Level 1C) or as surface reflectance (Level 2A). An extensive validation campaign was held to check the performances of these products with regard to the multi-temporal registration, the quality of cloud masks, the accuracy of aerosol optical thickness estimates and the quality of surface reflectances. Despite high a priori geo-location errors, it was possible to register the images with an accuracy better than 0.5 pixels in the large majority of cases. Despite the lack of a blue band on the SPOT-4 satellite, the cloud and shadow detection yielded good results, while the aerosol optical thickness was measured with a root mean square error better than 0.06. The surface reflectances after atmospheric correction were compared with in situ data and other satellite data showing little bias and the standard deviation of surface reflectance errors in the range (0.01-0.02). The Take 5 experiment is being repeated in 2015 with the SPOT-5 satellite with an enhanced resolution.
C1 [Hagolle, Olivier; Huc, Mireille] Univ Toulouse, Ctr Etud Spatiales Biosphere, CESBIO Unite Mixte, CNES CNRS IRD, F-31401 Toulouse 9, France.
[Sylvander, Sylvia; Dechoz, Cecile; Lonjou, Vincent] CNES, F-31401 Toulouse 9, France.
[Claverie, Martin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Clesse, Dominique] Capgemini Technol Serv, F-31036 Toulouse 1, France.
[Poulain, Vincent] Thales Serv, F-31400 Toulouse, France.
RP Hagolle, O (reprint author), Univ Toulouse, Ctr Etud Spatiales Biosphere, CESBIO Unite Mixte, CNES CNRS IRD, 18 Ave E Belin, F-31401 Toulouse 9, France.
EM olivier.hagolle@cesbio.cnes.fr; sylvia.sylvander@cnes.fr;
mireille.huc@cesbio.cnes.fr; martin.claverie@nasa.gov;
dominique.clesse@capgemini.com; cecile.dechoz@cnes.fr;
vincent.lonjou@cnes.fr; vincent.poulain@thalesgroup.com
NR 29
TC 15
Z9 15
U1 5
U2 10
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD SEP
PY 2015
VL 7
IS 9
BP 12242
EP 12264
DI 10.3390/rs70912242
PG 23
WC Remote Sensing
SC Remote Sensing
GA CT0UA
UT WOS:000362511400058
ER
PT J
AU Robinson, SB
Christian, JA
AF Robinson, Shane B.
Christian, John A.
TI Pattern Design for 3D Point Matching
SO NAVIGATION-JOURNAL OF THE INSTITUTE OF NAVIGATION
LA English
DT Article
ID CAPTURE; SPACE
AB This paper presents an approach for designing 3D point patterns which are uniquely distinguishable in the absence of an a priori pose estimate. The principles for designing 3D point patterns are presented. Simple example patterns with analytic solutions are used to illustrate the approach. The search for desirable point patterns is mechanized through the optimization of a fitness function. This fitness function provides a metric for assessing the distinguishability of any pattern. Two example applications are given to demonstrate the utility of the technique for navigation systems. Finally, the technique is modified to allow the use of evolutionary algorithms for the design of patterns having greater complexity. Published 2015. This article is a U.S. Government work and is in the public domain in the USA.
C1 [Robinson, Shane B.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Christian, John A.] W Virginia Univ, Morgantown, WV 26506 USA.
RP Robinson, SB (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 17
TC 1
Z9 1
U1 4
U2 4
PU WILEY PERIODICALS, INC
PI SAN FRANCISCO
PA ONE MONTGOMERY ST, SUITE 1200, SAN FRANCISCO, CA 94104 USA
SN 0028-1522
EI 2161-4296
J9 NAVIGATION-US
JI Navigation
PD FAL
PY 2015
VL 62
IS 3
BP 189
EP 203
DI 10.1002/navi.115
PG 15
WC Engineering, Aerospace; Remote Sensing; Telecommunications
SC Engineering; Remote Sensing; Telecommunications
GA CU9WY
UT WOS:000363898800002
ER
PT J
AU Cremades, H
Iglesias, FA
St Cyr, OC
Xie, H
Kaiser, ML
Gopalswamy, N
AF Cremades, H.
Iglesias, F. A.
St Cyr, O. C.
Xie, H.
Kaiser, M. L.
Gopalswamy, N.
TI Low-Frequency Type-II Radio Detections and Coronagraph Data Employed to
Describe and Forecast the Propagation of 71 CMEs/Shocks
SO SOLAR PHYSICS
LA English
DT Article
DE Coronal mass ejections, initiation and propagation; Radio bursts, type
II; Waves, shock
ID SOLAR-WIND STRUCTURES; SUN-EARTH CONNECTION; MASS EJECTIONS;
INTERPLANETARY SHOCKS; AERODYNAMIC DRAG; ARRIVAL TIMES; 1 AU;
ELECTRON-DENSITY; STEREO MISSION; DRIVEN SHOCKS
AB Motivated by improving predictions of arrival times at Earth of shocks driven by coronal mass ejections (CMEs), we have analyzed 71 Earth-directed events in different stages of their propagation. The study is primarily based on approximated locations of interplanetary (IP) shocks derived from Type-II radio emissions detected by the Wind/WAVES experiment during 1997 -aEuro parts per thousand 2007. Distance-time diagrams resulting from the combination of white-light corona, IP Type-II radio, and in-situ data lead to the formulation of descriptive profiles of each CME's journey toward Earth. Furthermore, two different methods for tracking and predicting the location of CME-driven IP shocks are presented. The linear method, solely based on Wind/WAVES data, arises after key modifications to a pre-existing technique that linearly projects the drifting low-frequency Type-II emissions to 1 AU. This upgraded method improves forecasts of shock-arrival times by almost 50 %. The second predictive method is proposed on the basis of information derived from the descriptive profiles and relies on a single CME height-time point and on low-frequency Type-II radio emissions to obtain an approximate value of the shock arrival time at Earth. In addition, we discuss results on CME-radio emission associations, characteristics of IP propagation, and the relative success of the forecasting methods.
C1 [Cremades, H.; Iglesias, F. A.] Univ Tecnol, Fac Reg Mendoza, Mendoza, Argentina.
[Cremades, H.] Consejo Nacl Invest Cient & Tecn, Buenos Aires, DF, Argentina.
[St Cyr, O. C.; Xie, H.; Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Xie, H.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Cremades, H (reprint author), Univ Tecnol, Fac Reg Mendoza, Mendoza, Argentina.
EM hebe.cremades@frm.utn.edu.ar; iglesias@mps.mpg.de; chris.stcyr@nasa.gov;
hong.xie@nasa.gov; michael.kaiser@rocketmail.com;
nat.gopalswamy@nasa.gov
FU Universidad Tecnologica Nacional - Facultad Regional Mendoza
[CONVPICT-PROM01 2007]; NASA's LWS TRT program [8-LWSTRT08-0029];
NASA/LWS program; AISRP program
FX H. Cremades and F.A. Iglesias acknowledge the funding of project
CONVPICT-PROM01 2007 of Universidad Tecnologica Nacional - Facultad
Regional Mendoza. H. Cremades is a member of the Carrera del
Investigador Cientifico (CONICET). O.C. St. Cyr, H. Xie, and N.
Gopalswamy gratefully acknowledge support from NASA's LWS TR&T program
through grant 8-LWSTRT08-0029. The authors thank Ernesto
Aguilar-Rodriguez and Craig Markwardt for their support on Solar Soft
and IDL routines, Cathie Meetre for guidance on neural-network usage for
automated density detection, Dibyendu Nandy for providing the full list
of CME events corrected by the HNK method, and Ivo Dohmen for
disinterested help, as well as the referee for helpful comments and
suggestions.; The SOHO/LASCO data are produced by an international
consortium of the NRL (USA), MPI fur Sonnensystemforschung (Germany),
Laboratoire d'Astronomie (France), and the University of Birmingham
(UK). SOHO is a project of international cooperation between ESA and
NASA. The STEREO/SECCHI project is an international consortium of the
NRL, LMSAL and NASA/GSFC (USA), RAL and Univ. Birmingham (UK), MPS
(Germany), CSL (Belgium), IOTA and IAS (France). SDO/AIA and SDO/HMI
data are courtesy of the NASA/SDO and the AIA and HMI Science Teams.
This article uses data from the SOHO/LASCO CME catalog generated and
maintained at the CDAW Data Center by NASA and the CUA in cooperation
with NRL, from the CACTus CME catalog generated and maintained by the
SIDC at the ROB, and the SEEDS project supported by the NASA/LWS and
AISRP programs.
NR 79
TC 5
Z9 5
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2015
VL 290
IS 9
BP 2455
EP 2478
DI 10.1007/s11207-015-0776-y
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU7MX
UT WOS:000363725300006
ER
PT J
AU Yu, HS
Jackson, BV
Hick, PP
Buffington, A
Odstrcil, D
Wu, CC
Davies, JA
Bisi, MM
Tokumaru, M
AF Yu, H. -S.
Jackson, B. V.
Hick, P. P.
Buffington, A.
Odstrcil, D.
Wu, C. -C.
Davies, J. A.
Bisi, M. M.
Tokumaru, M.
TI 3D Reconstruction of Interplanetary Scintillation (IPS) Remote-Sensing
Data: Global Solar Wind Boundaries for Driving 3D-MHD Models
SO SOLAR PHYSICS
LA English
DT Article
DE Interplanetary scintillation; Solar wind; 3D-MHD models; Remote sensing;
Forecasting
ID CORONAL MASS EJECTIONS; TIME-DEPENDENT TOMOGRAPHY; STEREO HELIOSPHERIC
IMAGERS; INNER HELIOSPHERE; MHD MODEL; NUMERICAL-SIMULATION; FIELD
ENHANCEMENTS; GEOMAGNETIC STORMS; COMPOUND STREAMS; EVOLUTION
AB The University of California, San Diego, time-dependent analyses of the heliosphere provide three-dimensional (3D) reconstructions of solar wind velocities and densities from observations of interplanetary scintillation (IPS). Using data from the Solar-Terrestrial Environment Laboratory, Japan, these reconstructions provide a real-time prediction of the global solar-wind density and velocity throughout the whole heliosphere with a temporal cadence of about one day ips.ucsd.edu . Updates to this modeling effort continue: in the present article, near-Sun results extracted from the time-dependent 3D reconstruction are used as inner boundary conditions to drive 3D-MHD models (e.g. ENLIL and H3D-MHD). This allows us to explore the differences between the IPS kinematic-model data-fitting procedure and current 3D-MHD modeling techniques. The differences in these techniques provide interesting insights into the physical principles governing the expulsion of coronal mass ejections (CMEs). Here we detail for the first time several specific CMEs and an induced shock that occurred in September 2011 that demonstrate some of the issues resulting from these analyses.
C1 [Yu, H. -S.; Jackson, B. V.; Hick, P. P.; Buffington, A.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Odstrcil, D.] George Mason Univ, Fairfax, VA 22030 USA.
[Odstrcil, D.] NASA, GSFC MC 674, Greenbelt, MD 20771 USA.
[Wu, C. -C.] Naval Res Lab, Washington, DC 20375 USA.
[Davies, J. A.; Bisi, M. M.] Rutherford Appleton Lab, Sci & Technol Facil Council, RAL Space, Didcot OX11 0QX, Oxon, England.
[Tokumaru, M.] Nagoya Univ, Solar Terrestrial Environm Lab STELab, Nagoya, Aichi 4648601, Japan.
RP Yu, HS (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr 0424, La Jolla, CA 92093 USA.
EM hsyu@ucsd.edu; bvjackson@ucsd.edu; pphick@ucsd.edu;
abuffington@ucsd.edu; dusanod@gmail.com; chin-chun.wu@nrl.navy.mil;
jackie.davies@stfc.ac.uk; mario.bisi@stfc.ac.uk;
tokumaru@stelab.nagoya-u.ac.jp
FU NSF [AGS-1053766, AGS-1358399]; AFOSR [FA9550-11-1-0324]; ONR 6.1
program; Center for Astrophysics and Space Sciences at UCSD; STELab,
Nagoya University
FX H.-S. Yu, B.V. Jackson, P.P. Hick, and A. Buffington were supported at
UCSD by NSF grants AGS-1053766, and AGS-1358399, and by AFOSR grant
FA9550-11-1-0324. Work of C.-C. Wu was supported by the ONR 6.1 program.
The authors wish to acknowledge and thank the group at STELab, Nagoya
University (those not included in the author list: M. Kojima, K. Fujiki,
and students) for their continued support, and for making IPS data sets
available under the auspices of a joint collaborative agreement between
the Center for Astrophysics and Space Sciences at UCSD and STELab,
Nagoya University. We wish to thank Kevin Schenk and the LASCO
coronagraph group for the CME images taken using the C2 coronagraph, and
the STEREO/SECCHI group for making available their COR2 images. We also
thank the UKSSDC (UK solar system data centre) for providing the HI
data.
NR 87
TC 4
Z9 4
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD SEP
PY 2015
VL 290
IS 9
BP 2519
EP 2538
DI 10.1007/s11207-015-0685-0
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CU7MX
UT WOS:000363725300010
ER
PT J
AU Pulkkinen, A
Mahmood, S
Ngwira, C
Balch, C
Lordan, R
Fugate, D
Jacobs, W
Honkonen, I
AF Pulkkinen, A.
Mahmood, S.
Ngwira, C.
Balch, C.
Lordan, R.
Fugate, D.
Jacobs, W.
Honkonen, I.
TI Solar Storm GIC Forecasting: Solar Shield Extension-Development of the
End-User Forecasting System Requirements
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE geomagnetically induced currents; forecasting
C1 [Pulkkinen, A.] NASA, Goddard Space Flight Ctr, Space Weather Res Ctr, Greenbelt, MD USA.
[Mahmood, S.] Sci & Technol Directorate, Dept Homeland Secur, Resilient Elect Grid Program, Washington, DC USA.
[Ngwira, C.] Catholic Univ Amer, Washington, DC 20064 USA.
[Balch, C.] NOAA, Space Weather Predict Ctr, Boulder, CO USA.
[Lordan, R.] Elect Power Res Inst, Palo Alto, CA USA.
[Fugate, D.; Jacobs, W.] Elect Res & Management, Cabot, PA USA.
[Honkonen, I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Pulkkinen, A (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Res Ctr, Greenbelt, MD USA.
EM antti.a.pulkkinen@nasa.gov
NR 5
TC 2
Z9 2
U1 0
U2 0
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 SEP
PY 2015
VL 13
IS 9
BP 531
EP 532
DI 10.1002/2015SW001283
PG 2
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA CU4ER
UT WOS:000363480300004
ER
PT J
AU MacDonald, EA
Case, NA
Clayton, JH
Hall, MK
Heavner, M
Lalone, N
Patel, KG
Tapia, A
AF MacDonald, E. A.
Case, N. A.
Clayton, J. H.
Hall, M. K.
Heavner, M.
Lalone, N.
Patel, K. G.
Tapia, A.
TI Aurorasaurus: A citizen science platform for viewing and reporting the
aurora
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE aurora; citizen science; alerts
ID ARC THICKNESSES; TWITTER; VOLUNTEERS; EARTHQUAKE; PROJECT; MODEL
AB A new, citizen science-based, aurora observing and reporting platform has been developed with the primary aim of collecting auroral observations made by the general public to further improve the modeling of the aurora. In addition, the real-time ability of this platform facilitates the combination of citizen science observations with auroral oval models to improve auroral visibility nowcasting. Aurorasaurus provides easily understandable aurora information, basic gamification, and real-time location-based notification of verified aurora activity to engage citizen scientists. The Aurorasaurus project is one of only a handful of space weather citizen science projects and can provide useful results for the space weather and citizen science communities. Early results are promising with over 2000 registered users submitting over 1000 aurora observations and verifying over 1700 aurora sightings posted on Twitter.
C1 [MacDonald, E. A.; Case, N. A.; Heavner, M.; Patel, K. G.] New Mexico Consortium, Los Alamos, NM USA.
[MacDonald, E. A.; Case, N. A.; Patel, K. G.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Clayton, J. H.; Hall, M. K.] Sci Educ Solut, Los Alamos, NM USA.
[Heavner, M.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Lalone, N.; Tapia, A.] Penn State Univ, Coll Informat Sci & Technol, University Pk, PA 16802 USA.
RP MacDonald, EA (reprint author), New Mexico Consortium, Los Alamos, NM USA.
EM e.a.macdonald@nasa.gov
OI Case, Nathan/0000-0003-0692-1778
FU National Science Foundation (NSF) [1344296]; Los Alamos National
Laboratory's Institute for Geophysics and Planetary Physics (IGPP);
Laboratory Directed R&D under the Van Allen Probes; Laboratory Directed
R&D under the NASA Goddard
FX This material is based upon the work supported, in part, by the National
Science Foundation (NSF) under grant 1344296. Any opinions, findings,
and conclusions or recommendations expressed in this material are those
of the author(s) and do not necessarily reflect the views of NSF.
Additional support has been provided by strategic investments by Los
Alamos National Laboratory's Institute for Geophysics and Planetary
Physics (IGPP) and Laboratory Directed R&D funding, NASA EPO under the
Van Allen Probes, and NASA Goddard. We gratefully acknowledge the NOAA
SWPC as the provider of real-time space weather data for the nation. We
would like to thank Dirk Lummerzheim (UAF) for sharing a version of the
UAF aurora model with us. We are grateful to the volunteer members of
the Aurorasaurus Scientist Network and the Aurorasaurus Advisory Board.
Software development and support has been provided by Ideum, David
Kingman, Social Flow, and others. Reid Priedhorsky, Yan Cao, and Niels
van Hecke were critical for prototype development. The New Mexico
Consortium has provided multilateral administrative support.
NR 57
TC 2
Z9 2
U1 2
U2 16
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 SEP
PY 2015
VL 13
IS 9
BP 548
EP 559
DI 10.1002/2015SW001214
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA CU4ER
UT WOS:000363480300007
ER
PT J
AU Joyce, CJ
Schwadron, NA
Townsend, LW
Mewaldt, RA
Cohen, CMS
von Rosenvinge, TT
Case, AW
Spence, HE
Wilson, JK
Gorby, M
Quinn, M
Zeitlin, CJ
AF Joyce, C. J.
Schwadron, N. A.
Townsend, L. W.
Mewaldt, R. A.
Cohen, C. M. S.
von Rosenvinge, T. T.
Case, A. W.
Spence, H. E.
Wilson, J. K.
Gorby, M.
Quinn, M.
Zeitlin, C. J.
TI Analysis of the potential radiation hazard of the 23 July 2012 SEP event
observed by STEREO A using the EMMREM model and LRO/CRaTER
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE Radiation; Modeling; ICME
ID CORONAL MASS EJECTION; SOLAR EVENTS; MISSION; VALIDATION; SIMULATION;
PARTICLES; SPECTRA
AB We present a study of the potential radiation hazard of the powerful, superfast interplanetary coronal mass ejection (ICME) observed by STEREO A on 23 July 2012. Using energetic proton flux data from the High Energy Telescope and Low Energy Telescope instruments aboard STEREO A together with the Earth-Moon-Mars Radiation Environment Module, we compute dose rates and accumulated doses during the event for both skin/eye and blood forming organs using four physically relevant levels of shielding. For spacesuit equivalent shielding, we compute a peak skin/eye dose rate of 1970 cGy-Eq/d, a value far greater than those of the 2003 Halloween storms or the January and March solar energetic particle events of 2012. However, due to the relative brevity of the event, the resulting accumulated dose was just 383 cGy-Eq, which is more aligned with the total doses of the 2003 Halloween and 2012 January/March events. Additionally, we use dose rates at STEREO B and Lunar Reconnaissance Orbiter/Cosmic Ray Telescope for the Effects of Radiation (LRO/CRaTER) during the event to show how the radiation impact is affected by the position of the ICME relative to the observer. Specifically, we find that the energetic particle event associated with the local shock and ICME passage at STEREO A caused greatly enhanced dose rates when compared to STEREO B and LRO/CRaTER, which were longitudinally distant from the ICME. The STEREO A/B dose rates used here will soon be made available to the community as a tool for studying the energetic particle radiation of solar events from different longitudes as a part of NASA's Heliophysics Virtual Observatories and on the Predictions of radiation from REleASE, EMMREM, and Data Incorporating CRaTER, COSTEP, and other SEP measurements (PREDICCS) and CRaTER websites.
C1 [Joyce, C. J.; Schwadron, N. A.; Spence, H. E.; Wilson, J. K.; Gorby, M.; Quinn, M.] Univ New Hampshire, Ctr Space Sci, Dept Phys, Durham, NH 03824 USA.
[Townsend, L. W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA.
[Mewaldt, R. A.; Cohen, C. M. S.] CALTECH, Pasadena, CA 91125 USA.
[von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
[Case, A. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zeitlin, C. J.] SW Res Inst, Boulder, CO USA.
RP Joyce, CJ (reprint author), Univ New Hampshire, Ctr Space Sci, Dept Phys, Durham, NH 03824 USA.
EM cjl46@unh.edu
FU NASA LRO/CRaTER/PREDICCS Project [NNG11PA03C]; NSF/FESD Sun-to-Ice
Project [AGS1135432]; NASA/LWS/NSF EMMREM Project [NNX11AC06G]; NASA
[NNX11A075G]; UC Berkeley under NASA [SA2715-26309, NAS5-003131]
FX This work is supported by NASA LRO/CRaTER/PREDICCS Project (contract
NNG11PA03C), the NSF/FESD Sun-to-Ice Project (grant AGS1135432), and the
NASA/LWS/NSF EMMREM Project (grant NNX11AC06G). The work on the
corrected STEREO A HET spectrum was performed at Caltech and was
supported by NASA grants NNX11A075G and subcontract SA2715-26309 from UC
Berkeley under NASA Contract NAS5-003131. We thank the STEREO HET and
LET instrument teams for providing the STEREO data used here (available
at:http://www.srl.caltech.edu/STEREO/). Simulation results have been
provided by the Community Coordinated Modeling Center at Goddard Space
Flight Center through their public Runs on Request system
((http://ccmc.gsfc.nasa.gov). The CCMC is a multiagency partnership
between NASA, AFMC, AFOSR, AFRL, AFWA, NOAA, NSF, and ONR. The
ENLIL+Cone Model was developed by Dusan Odstrcil at the University of
Colorado at Boulder. The CRaTER data used here are available on the
CRaTER website:http://crater-web.sr.unh.edu/.
NR 26
TC 2
Z9 2
U1 2
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD SEP
PY 2015
VL 13
IS 9
BP 560
EP 567
DI 10.1002/2015SW001208
PG 8
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA CU4ER
UT WOS:000363480300008
ER
PT J
AU McDonald, SE
Sassi, F
Mannucci, AJ
AF McDonald, S. E.
Sassi, F.
Mannucci, A. J.
TI SAMI3/SD-WACCM-X simulations of ionospheric variability during northern
winter 2009
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE ionospheric modeling; lower atmospheric coupling; SSW
ID LOWER THERMOSPHERE; SEASONAL-VARIATION; DIURNAL TIDE; WACCM-X;
ATMOSPHERE; MODEL; MESOSPHERE; WAVE; GCM
AB We have performed simulations using the Naval Research Laboratory's physics-based model of the ionosphere, Sami3 is A Model of the Ionosphere (SAMI3), to illustrate how neutral wind dynamics is responsible for day-to-day variability of the ionosphere. We have used neutral winds specified from the extended version of the specified dynamics Whole Atmosphere Community Climate Model (SD-WACCM-X), in which meteorology below 92km is constrained by atmospheric specifications from an operational weather forecast model and reanalysis. To assess the realism of the simulations against observations, we have carried out a case study during January-February 2009, a dynamically disturbed time characterized by a sudden stratospheric warming (SSW) commencing 24 January 2009. Model results are compared with total electron content (TEC) from Jet Propulsion Laboratory global ionospheric maps. We show that SAMI3/SD-WACCM-X captures longitudinal variability in the equatorial ionization anomaly associated with nonmigrating tides, with strongest contributions coming from the diurnal eastward wave number 2 (DE2) and DE3. Both migrating and nonmigrating tides contribute to significant day-to-day variability, with TEC varying up to 16%. Our simulation during the SSW period reveals that at the Jicamarca longitude (285 degrees E) on 27 January 2009 nonmigrating tides contribute to an enhancement of the electron density in the morning followed by a decrease in the afternoon. An enhancement of the semidiurnal eastward wave number 2 (SE2) and SE3 nonmigrating tides, likely associated with the appearance of the SSW, suggests that these tides increase the longitudinal variability of the SSW impact on the ionosphere. The conclusion is that realistic meteorology propagating upward from the lower atmosphere influences the dynamo region and reproduces aspects of the observed variability in the ionosphere.
C1 [McDonald, S. E.; Sassi, F.] Naval Res Lab, Div Space Sci, Washington, DC USA.
[Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP McDonald, SE (reprint author), Naval Res Lab, Div Space Sci, Washington, DC USA.
EM sarah.mcdonald@nrl.navy.mil
FU Chief of Naval Research through NRL; NASA/LWS [NNH12AT21I]; Heliophysics
Division of NASA's Science Mission Directorate
FX SAMI3 and SD-WACCM-X simulation output is archived at the Naval Research
Laboratory. Global ionospheric maps of TEC are maintained by JPL. The
Scherliess-Fejer model is available upon request from Ludgar Scherliess
at Utah State University. Model output and TEC data sets are available
from the authors upon request. S.M. and F.S. are supported by the Chief
of Naval Research through NRL base funding. F.S. was partially supported
by NASA/LWS grant NNH12AT21I. This work was also supported in part by a
grant of computer time from the DOD High Performance Computing
Modernization Program at the U.S. Navy DOD Supercomputing Resource
Center (NAVO). 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.
Sponsorship of the Heliophysics Division of NASA's Science Mission
Directorate is gratefully acknowledged. Finally, we would like to thank
Joseph Huba for providing us with the SAMI3 source code.
NR 75
TC 5
Z9 5
U1 3
U2 9
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 SEP
PY 2015
VL 13
IS 9
BP 568
EP 584
DI 10.1002/2015SW001223
PG 17
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA CU4ER
UT WOS:000363480300009
ER
PT J
AU Wang, SG
Sobel, AH
Fridlind, A
Feng, Z
Comstock, JM
Minnis, P
Nordeen, ML
AF Wang, Shuguang
Sobel, Adam H.
Fridlind, Ann
Feng, Zhe
Comstock, Jennifer M.
Minnis, Patrick
Nordeen, Michele L.
TI Simulations of cloud-radiation interaction using large-scale forcing
derived from the CINDY/DYNAMO northern sounding array
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; TEMPERATURE-GRADIENT APPROXIMATION; TROPICAL
INTRASEASONAL OSCILLATION; RESOLVING MODEL SIMULATIONS; STATIC ENERGY
BUDGET; OCEAN MIXED-LAYER; INDIAN-OCEAN; TOGA COARE; PART I; STRATIFORM
PRECIPITATION
AB The recently completed CINDY/DYNAMO field campaign observed two Madden-Julian oscillation (MJO) events in the equatorial Indian Ocean from October to December 2011. Prior work has indicated that the moist static energy anomalies in these events grew and were sustained to a significant extent by radiative feedbacks. We present here a study of radiative fluxes and clouds in a set of cloud-resolving simulations of these MJO events. The simulations are driven by the large-scale forcing data set derived from the DYNAMO northern sounding array observations, and carried out in a doubly periodic domain using the Weather Research and Forecasting (WRF) model. Simulated cloud properties and radiative fluxes are compared to those derived from the S-PolKa radar and satellite observations. To accommodate the uncertainty in simulated cloud microphysics, a number of single-moment (1M) and double-moment (2M) microphysical schemes in the WRF model are tested. The 1M schemes tend to underestimate radiative flux anomalies in the active phases of the MJO events, while the 2M schemes perform better, but can overestimate radiative flux anomalies. All the tested microphysics schemes exhibit biases in the shapes of the histograms of radiative fluxes and radar reflectivity. Histograms of radiative fluxes and brightness temperature indicate that radiative biases are not evenly distributed; the most significant bias occurs in rainy areas with OLR less than 150 W/m(2) in the 2M schemes. Analysis of simulated radar reflectivities indicates that this radiative flux uncertainty is closely related to the simulated stratiform cloud coverage. Single-moment schemes underestimate stratiform cloudiness by a factor of 2, whereas 2M schemes simulate much more stratiform cloud.
C1 [Wang, Shuguang; Sobel, Adam H.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
[Sobel, Adam H.] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA.
[Sobel, Adam H.] Columbia Univ, Dept Earth & Environm Sci, New York, NY USA.
[Fridlind, Ann] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Feng, Zhe; Comstock, Jennifer M.] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Nordeen, Michele L.] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Wang, SG (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
EM sw2526@columbia.edu
RI Wang, Shuguang/C-2893-2011; Sobel, Adam/K-4014-2015; Feng,
Zhe/E-1877-2015
OI Wang, Shuguang/0000-0003-1861-9285; Sobel, Adam/0000-0003-3602-0567;
Feng, Zhe/0000-0002-7540-9017
FU NSF [AGS-1062206]; Department of Energy Atmospheric Science Research
Program [DE-SC0000991/006]; U.S. Department of Energy (DOE), Office of
Biological and Environmental Research, as part of the Atmospheric System
Research (ASR) Program; DOE [DE-AC05-76RL01830]
FX S.W. and A.H.S. were supported by NSF grant AGS-1062206. We would like
to thank two anonymous reviewers for the insightful comments. We thank
Scott Powell and Manuel Zuluaga for their clarification of the
convective/stratiform analysis and Hannah Barnes for the discussion on
the observed microphysical structures. The CERES-SYN1deg data were
provided by the CERES team via their webpage:
http://ceres.larc.nasa.gov/products.php?product=SYN1deg. The research
used data from the Atmospheric Radiation Measurement Climate Research
Facility, A DOE Office of Science User Facility, and can be accessed
with the data doi:10.5439/1134823 (http://dx.doi.org/10.5439/1169498).
Thanks to R. Palikonda and M. Khaiyer for assistance in the analysis of
FY-2E data, which was supported by the Department of Energy Atmospheric
Science Research Program under Interagency Agreement DE-SC0000991/006.
The Pacific Northwest National Laboratory authors are supported by the
U.S. Department of Energy (DOE), Office of Biological and Environmental
Research, as part of the Atmospheric System Research (ASR) Program. The
Pacific Northwest National Laboratory is operated for DOE by Battelle
Memorial Institute under contract DE-AC05-76RL01830.
NR 129
TC 3
Z9 3
U1 2
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PD SEP
PY 2015
VL 7
IS 3
BP 1472
EP 1498
DI 10.1002/2015MS000461
PG 27
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU1JV
UT WOS:000363278200027
ER
PT J
AU Urquhart, EA
Zaitchik, BF
Guikema, SD
Haley, BJ
Taviani, E
Chen, A
Brown, ME
Huq, A
Colwell, RR
AF Urquhart, E. A.
Zaitchik, B. F.
Guikema, S. D.
Haley, B. J.
Taviani, E.
Chen, A.
Brown, M. E.
Huq, A.
Colwell, R. R.
TI Use of Environmental Parameters to Model Pathogenic Vibrios in
Chesapeake Bay
SO JOURNAL OF ENVIRONMENTAL INFORMATICS
LA English
DT Article
DE quantitative colony bot hybridization; hybrid modeling; classification;
regression; generalized additive model; random forest model
ID COAST OYSTERS; PARAHAEMOLYTICUS; VULNIFICUS; SALINITY; CHOLERAE; GULF;
EPIDEMIOLOGY; TEMPERATURE; INFECTIONS
AB Annual reports show that human infections caused by Vibrio spp. have nearly doubled over the past decade in the Virginia and Maryland waters of the Chesapeake Bay. Vibrio spp. are autochthonous to estuarine and coastal waters and follow a seasonal cycle attributed mainly to fluctuations in water temperature and salinity. This study presents the development of empirical algorithms for predicting the probability of Vibrio vulnificus and Vibrio parahaemolyticus likelihood and abundance in the upper Chesapeake Bay. To model likelihood of occurrence, a set of binary classification models was developed, employing a suite of geophysical predictor variables and statistical methods. Accuracy of results was similar to 68% at 0.40 prediction for V. vulnificus and similar to 70% at 0.60 prediction for V parahaemolyticus. For Vibrio spp. abundance, regression methods were applied to samples positive for Vibrio, showing Vibrio abundance can be predicted as a function of sea surface temperature and salinity in Chesapeake Bay, with mean absolute error (MAE) of 3.9 cells 10 ml(-1) for V vulnificus and 5.8 cells 10 ml(-1) for V parahaemolyticus. Additionally, for the purpose of operational potential in the Chesapeake Bay, we developed a two-step classification/regression hybrid approach was used to generate estimates of abundance in the absence of bacteriological data on presence of Vibrio spp. This hybrid approach predicted Vibrio abundance with MAE of 2.8 cells 10 ml(-1) for V vulnificus and 4.4 cells 10(-1) ml for V parahaemolyticus. Since the risk of human infection is a function of Vibrio spp. pathogenicity and abundance, extending available predictive modeling capabilities to provide concentration, in addition to presence/absence, advances the public health utility of these models significantly.
C1 [Urquhart, E. A.; Zaitchik, B. F.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Guikema, S. D.] Johns Hopkins Univ, Dept Geog & Environm Engn, Baltimore, MD 21218 USA.
[Haley, B. J.; Taviani, E.; Chen, A.; Huq, A.] Univ Maryland, Maryland Pathogen Res Inst, Dept Mol Genet & Cell Biol, College Pk, MD 20742 USA.
[Brown, M. E.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Colwell, R. R.] Univ Maryland, Ctr Bioinformat & Computat Biol, UMIACS, College Pk, MD 20742 USA.
RP Urquhart, EA (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
EM erin.urquhart@unh.edu
RI Urquhart, Erin/A-2336-2015
OI Urquhart, Erin/0000-0001-7141-9499
FU Johns Hopkins University Department of Earth and Planetary Sciences;
NASA Headquarters Applied Sciences Division; National Institutes of
Health [2RO1A1039129-11A2]; National Science Foundation [0813066]
FX This study was funded in part by the Johns Hopkins University Department
of Earth and Planetary Sciences and by a grant from the NASA
Headquarters Applied Sciences Division. The authors would like to thank
the Maryland Department of Natural Resources, Chesapeake Bay Program,
and NASA GEO-CAPE field campaigns for allowing sample collection upon
routine Bay cruises as well as Valerie Cohen and Merina Elahi (MPRI,
UMCP) for wet lab assistance. The authors gratefully acknowledge partial
support at the Maryland Pathogen Research Institute at the University of
Maryland, College Park, from National Institutes of Health Grant No.
2RO1A1039129-11A2 and National Science Foundation Grant No. 0813066.
NR 39
TC 3
Z9 3
U1 1
U2 16
PU INT SOC ENVIRON INFORM SCI
PI REGINA
PA 4246 ALBERT ST, REGINA, SASKATCHEWAN S4S 3R9, CANADA
SN 1726-2135
EI 1684-8799
J9 J ENVIRON INFORM
JI J. Environ. Inform.
PD SEP
PY 2015
VL 26
IS 1
BP 1
EP 13
DI 10.3808/jei.201500307
PG 13
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA CU2LM
UT WOS:000363355000001
ER
PT J
AU Anav, A
Friedlingstein, P
Beer, C
Ciais, P
Harper, A
Jones, C
Murray-Tortarolo, G
Papale, D
Parazoo, NC
Peylin, P
Piao, SL
Sitch, S
Viovy, N
Wiltshire, A
Zhao, MS
AF Anav, Alessandro
Friedlingstein, Pierre
Beer, Christian
Ciais, Philippe
Harper, Anna
Jones, Chris
Murray-Tortarolo, Guillermo
Papale, Dario
Parazoo, Nicholas C.
Peylin, Philippe
Piao, Shilong
Sitch, Stephen
Viovy, Nicolas
Wiltshire, Andy
Zhao, Maosheng
TI Spatiotemporal patterns of terrestrial gross primary production: A
review
SO REVIEWS OF GEOPHYSICS
LA English
DT Review
DE GPP; DGVMs; ESMs; satellite; MTE
ID NET PRIMARY PRODUCTION; EARTH SYSTEM MODEL; ENVIRONMENT SIMULATOR JULES;
GENERAL-CIRCULATION MODEL; DROUGHT-INDUCED REDUCTION; GLOBAL VEGETATION
MODELS; CARBON-DIOXIDE EXCHANGE; LIGHT-USE EFFICIENCY; RAIN-FOREST TREE;
CHLOROPHYLL FLUORESCENCE
AB Great advances have been made in the last decade in quantifying and understanding the spatiotemporal patterns of terrestrial gross primary production (GPP) with ground, atmospheric, and space observations. However, although global GPP estimates exist, each data set relies upon assumptions and none of the available data are based only on measurements. Consequently, there is no consensus on the global total GPP and large uncertainties exist in its benchmarking. The objective of this review is to assess how the different available data sets predict the spatiotemporal patterns of GPP, identify the differences among data sets, and highlight the main advantages/disadvantages of each data set. We compare GPP estimates for the historical period (1990-2009) from two observation-based data sets (Model Tree Ensemble and Moderate Resolution Imaging Spectroradiometer) to coupled carbon-climate models and terrestrial carbon cycle models from the Fifth Climate Model Intercomparison Project and TRENDY projects and to a new hybrid data set (CARBONES). Results show a large range in the mean global GPP estimates. The different data sets broadly agree on GPP seasonal cycle in terms of phasing, while there is still discrepancy on the amplitude. For interannual variability (IAV) and trends, there is a clear separation between the observation-based data that show little IAV and trend, while the process-based models have large GPP variability and significant trends. These results suggest that there is an urgent need to improve observation-based data sets and develop carbon cycle modeling with processes that are currently treated either very simplistically to correctly estimate present GPP and better quantify the future uptake of carbon dioxide by the world's vegetation.
C1 [Anav, Alessandro; Friedlingstein, Pierre; Harper, Anna; Murray-Tortarolo, Guillermo] Univ Exeter, Coll Engn Math & Phys Sci, Exeter, Devon, England.
[Beer, Christian] Stockholm Univ, Dept Appl Environm Sci ITM, S-10691 Stockholm, Sweden.
[Beer, Christian] Stockholm Univ, Bolin Ctr Climate Res, S-10691 Stockholm, Sweden.
[Ciais, Philippe; Peylin, Philippe; Viovy, Nicolas] Lab Sci Climat & Environm, Gif Sur Yvette, France.
[Jones, Chris; Wiltshire, Andy] Met Off, Hadley Ctr, Exeter, Devon, England.
[Papale, Dario] Univ Tuscia, Dept Innovat Biol Agrofood & Forest Syst, Viterbo, Italy.
[Papale, Dario] CzechGlobe Global Change Res Ctr AS CR, Brno, Czech Republic.
[Parazoo, Nicholas C.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Piao, Shilong] Chinese Acad Sci, Inst Tibetan Plateau Res, Key Lab Alpine Ecol & Biodivers, Beijing, Peoples R China.
[Sitch, Stephen] Univ Exeter, Coll Life & Environm Sci, Exeter, Devon, England.
[Zhao, Maosheng] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
RP Anav, A (reprint author), Univ Exeter, Coll Engn Math & Phys Sci, Exeter, Devon, England.
EM A.Anav@exeter.ac.uk
RI Beer, Christian/D-2296-2013; Vuichard, Nicolas/A-6629-2011;
Friedlingstein, Pierre/H-2700-2014; Jones, Chris/I-2983-2014
FU European Commission [238366, 282672]; Joint DECC/Defra Met Office Hadley
Centre Climate Program [GA01101]
FX We acknowledge the World Climate Research Programme's Working Group on
Coupled Modeling, which is responsible for CMIP, and we thank the
climate modeling groups (listed in Table 1 of this paper) for producing
and making available their model output. For CMIP the U.S. Department of
Energy's Program for Climate Model Diagnosis and Intercomparison
provides coordinating support and led development of software
infrastructure in partnership with the Global Organization for Earth
System Science Portals. We thank also the principal investigators of the
eddy covariance sites responsible for the measurements and the whole
FLUXNET community. Data used in this work can be downloaded from the
European database at www.europe-fluxdata.eu. We also thank M. Reichstein
and M. Jung for providing MTE-GPP data through the site:
https://www.bgc-jena.mpg.de/bgi/index.php/Services/Overview, as well as
the Eumetsat for the GOME-2 data (http://avdc.gsfc.nasa.gov). CMIP5 data
can be freely downloaded from the following link:
http://pcmdi9.llnl.gov/esgf-web-fe/, while information on how to
retrieve TRENDY outputs are given in http://dgvm.ceh.ac.uk/node/9. MODIS
GPP data can be downloaded from the following link:
http://ntsg.umt.edu/. Finally, outputs from CARBONES are at
http://www.carbones.eu/wcmqs/. This work was supported by the European
Commission's Seventh Framework Programme under grant agreement 238366
(GREENCYCLESII) and 282672 (EMBRACE), while Jones was supported by the
Joint DECC/Defra Met Office Hadley Centre Climate Program (GA01101). We
also wish to thank Gregory Okin and two anonymous reviewers for their
positive comments on this manuscript.
NR 161
TC 26
Z9 26
U1 29
U2 80
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 8755-1209
EI 1944-9208
J9 REV GEOPHYS
JI Rev. Geophys.
PD SEP
PY 2015
VL 53
IS 3
BP 785
EP 818
DI 10.1002/2015RG000483
PG 34
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CU2GY
UT WOS:000363343200006
ER
PT J
AU Palmsten, ML
Kozarek, JL
Calantoni, J
AF Palmsten, Margaret L.
Kozarek, Jessica L.
Calantoni, Joseph
TI Video observations of bed form morphodynamics in a meander bend
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE Bed load; bed forms; bed form migration; sediment flux; meander bend
ID LARGE-SCALE; SEDIMENT TRANSPORT; BEDFORM MIGRATION; SAND-BED; RIVER;
RIPPLES; DUNES; MODEL; VELOCIMETRY; DYNAMICS
AB A new optical remote sensing technique for estimating water depth from an oblique camera view is described. The water surface and the bed were imaged simultaneously to create time-dependent maps of the water surface velocities and the bed elevations that can be used to validate numerical models at high spatial and temporal resolution. The technique was applied in a sandy meander bend at the University of Minnesota Saint Anthony Falls Laboratory Outdoor StreamLab. The root mean square differences between optical estimates of the bed and in situ observations ranged between 0.01 and 0.03 m. Mean bed form wavelength was 0.73 m and mean crest height was 0.07 m, but both varied with distance around the meander bend. Bed form classification varied with distance downstream, and sinuosity of bed forms varied with local radius of curvature. Bed form roughness scaled similarly to other natural riverine environments although wavelength and height magnitude and variability were larger than predicted by empirical formulations for straight reaches. Bed form translation rate varied between 1 and 5 mm s(-1). Estimates of velocity from particle image velocimetry (PIV) on the water surface were approximate to 10% higher than in situ observations collected approximate to 0.05 m below the water surface. Using the PIV observations to drive simple equations for bed load sediment flux, we explained up to 72% of the observed variance in downstream sediment flux. The new methodology described here provides nonintrusive, high spatial and temporal resolution measurements of both the bed and the flow.
C1 [Palmsten, Margaret L.; Calantoni, Joseph] Stennis Space Ctr, Naval Res Lab, Marine Geosci Div, Pearlington, MS 39572 USA.
[Kozarek, Jessica L.] Univ Minnesota, St Anthony Falls Lab, Minneapolis, MN USA.
RP Palmsten, ML (reprint author), Stennis Space Ctr, Naval Res Lab, Marine Geosci Div, Pearlington, MS 39572 USA.
EM 7434@nrlssc.navy.mil
FU Office of Naval Research; Science and Technology Center program of the
National Science Foundation (NSF) via National Center for Earth-surface
Dynamics [EAR-0120914]; National Cooperative Highway Research Program
[24-33]
FX Much of the data described here are presented in the supporting
information, additional data may be obtain with written permission from
the US Naval Research Laboratory. This work was performed while M.
Palmsten held a National Research Council Research Associateship Award
at the Naval Research Laboratory. J. Calantoni was supported under base
funding to the Naval Research Laboratory from the Office of Naval
Research. This work was partially supported by the Science and
Technology Center program of the National Science Foundation (NSF) via
the National Center for Earth-surface Dynamics under agreement number
EAR-0120914 and by the National Cooperative Highway Research Program
under project 24-33.The authors wish to thank the staff of the
University of Minnesota Saint Anthony Falls Stream Laboratory, as well
as T. Kooney for data collection efforts, and C. Chickadel, J.
Bartholdy, and an anonymous reviewer for their help improving the
manuscript. Any opinions, findings, and conclusions or recommendations
expressed in this material are solely those of the authors.
NR 58
TC 2
Z9 2
U1 4
U2 16
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD SEP
PY 2015
VL 51
IS 9
BP 7238
EP 7257
DI 10.1002/2014WR016321
PG 20
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA CU2YZ
UT WOS:000363391300019
ER
PT J
AU Lettenmaier, DP
Alsdorf, D
Dozier, J
Huffman, GJ
Pan, M
Wood, EF
AF Lettenmaier, Dennis P.
Alsdorf, Doug
Dozier, Jeff
Huffman, George J.
Pan, Ming
Wood, Eric F.
TI Inroads of remote sensing into hydrologic science during the WRR era
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE remote sensing; hydrological cycles and budgets; water budgets
ID SYNTHETIC-APERTURE RADAR; SNOW WATER EQUIVALENT; GLOBAL PRECIPITATION
MEASUREMENT; PASSIVE MICROWAVE MEASUREMENTS; STATIONS HYDRAULIC
GEOMETRY; SOIL-MOISTURE RETRIEVALS; LANDSAT THEMATIC MAPPER; ENSEMBLE
KALMAN FILTER; SIR-C/X-SAR; DATA ASSIMILATION
AB The first issue of WRR appeared eight years after the launch of Sputnik, but by WRR's 25(th) anniversary, only seven papers that used remote sensing had appeared. Over the journal's second 25 years, that changed remarkably, and remote sensing is now widely used in hydrology and other geophysical sciences. We attribute this evolution to production of data sets that scientists not well versed in remote sensing can use, and to educational initiatives like NASA's Earth System Science Fellowship program that has supported over a thousand scientists, many in hydrology. We review progress in remote sensing in hydrology from a water balance perspective. We argue that progress is primarily attributable to a creative use of existing and past satellite sensors to estimate such variables as evapotranspiration rates or water storage in lakes and reservoirs and to new and planned missions. Recent transforming technologies include the Gravity Recovery and Climate Experiment (GRACE), the European Soil Moisture and Ocean Salinity (SMOS) and U.S. Soil Moisture Active Passive (SMAP) missions, and the Global Precipitation Measurement (GPM) mission. Future missions include Surface Water and Ocean Topography (SWOT) to measure river discharge and lake, reservoir, and wetland storage. Measurement of some important hydrologic variables remains problematic: retrieval of snow water equivalent (SWE) from space remains elusive especially in mountain areas, even though snow cover extent is well observed, and was the topic of 4 of the first 5 remote sensing papers published in WRR. We argue that this area deserves more strategic thinking from the hydrology community.
C1 [Lettenmaier, Dennis P.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA.
[Alsdorf, Doug] Ohio State Univ, Byrd Polar & Climate Res Ctr, Columbus, OH 43210 USA.
[Dozier, Jeff] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA.
[Huffman, George J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pan, Ming; Wood, Eric F.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
RP Lettenmaier, DP (reprint author), Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA.
EM dlettenm@ucla.edu
RI Pan, Ming/B-6841-2011; Huffman, George/F-4494-2014;
OI Pan, Ming/0000-0003-3350-8719; Huffman, George/0000-0003-3858-8308;
Dozier, Jeff/0000-0001-8542-431X
FU NASA Earth Science; NOAA's Climate Program Office; Microsoft Research;
National Science Foundation
FX The work reported herein has been supported by multiple grants to the
authors from NASA Earth Science, NOAA's Climate Program Office,
Microsoft Research, and the National Science Foundation. We gratefully
acknowledge the assistance of Elizabeth Clark and Colin Gleason at UCLA,
Mike Durand at Ohio State University, Huilin Gao and Shuai Zhang at
Texas A&M University, and Faisal Hossain at the University of Washington
for assistance with preparation or modification of figures, and/or
comments on earlier versions of the text.
NR 228
TC 15
Z9 15
U1 16
U2 63
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD SEP
PY 2015
VL 51
IS 9
BP 7309
EP 7342
DI 10.1002/2015WR017616
PG 34
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA CU2YZ
UT WOS:000363391300023
ER
PT J
AU David, CH
Famiglietti, JS
Yang, ZL
Eijkhout, V
AF David, Cedric H.
Famiglietti, James S.
Yang, Zong-Liang
Eijkhout, Victor
TI Enhanced fixed-size parallel speedup with the Muskingum method using a
trans-boundary approach and a large subbasins approximation
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE trans-boundary; Muskingum; parallel; speedup; network; decomposition
ID SCALE RIVER FLOW; HYDROLOGICAL MODEL; SURFACE-WATER; NETWORKS; BALANCE;
SYSTEM; BASIN; CODIFICATION; SIMULATIONS; PARAMETERS
AB This study presents a new algorithm for parallel computation of river flow that builds on recent work demonstrating the relative independence of distant river reaches in the update step of the Muskingum method. The algorithm is designed to achieve enhanced fixed-size parallel speedup and uses a mathematical approximation applied at the boundaries of large subbasins. In order to use such an algorithm, a balanced domain decomposition method that differs from the traditional classifications of river reaches and subbasins and based on network topology is developed. An application of the algorithm and domain decomposition method to the Mississippi River Basin results in an eightfold decrease in computing time with 16 computing cores which is unprecedented for Muskingum-type algorithms applied in classic parallel-computing paradigms having a one-to-one relationship between cores and subbasins. An estimated 300 km between upstream and downstream reaches of subbasins guarantees the applicability of the algorithm in our study and motivates further investigation of domain decomposition methods.
C1 [David, Cedric H.; Famiglietti, James S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[David, Cedric H.; Famiglietti, James S.] Univ Calif Irvine, Ctr Hydrol Modeling, Irvine, CA USA.
[Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Yang, Zong-Liang] Univ Texas Austin, Dept Geol Sci, Jackson Sch Geosci, Austin, TX USA.
[Eijkhout, Victor] Univ Texas Austin, Texas Adv Comp Ctr, Austin, TX 78712 USA.
RP David, CH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM cedric.david@jpl.nasa.gov
RI Yang, Zong-Liang/B-4916-2011
FU University of California Office of President Multicampus Research
Programs and Initiatives; Jet Propulsion Laboratory, California
Institute of Technology; National Aeronautics and Space Administration
FX This work was supported by the University of California Office of the
President Multicampus Research Programs and Initiatives and by the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration; both
institutions are gratefully acknowledged. The practical application in
this study was made possible using the following freely available data:
river network information from the Hydrological data and maps based on
SHuttle Elevation Derivatives at multiple Scales (HydroSHEDS), estimates
of runoff from phase 2 of the North American Land Data Assimilation
System (NLDAS2) and gauge observations from the U.S. Geological Survey
National Water Information System (NWIS). The authors are thankful to
the Editor, Associate Editor, Reed Maxwell, Ezio Todini, and one
anonymous reviewer for their valuable comments on earlier versions of
this manuscript.
NR 72
TC 1
Z9 1
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD SEP
PY 2015
VL 51
IS 9
BP 7547
EP 7571
DI 10.1002/2014WR016650
PG 25
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA CU2YZ
UT WOS:000363391300035
ER
PT J
AU Murphy, TE
Kapili, BJ
Detweiler, AM
Bebout, BM
Prufert-Bebout, LE
AF Murphy, Thomas E.
Kapili, Bennett J.
Detweiler, Angela M.
Bebout, Brad M.
Prufert-Bebout, Leslie E.
TI Vertical distribution of algal productivity in open pond raceways
SO ALGAL RESEARCH-BIOMASS BIOFUELS AND BIOPRODUCTS
LA English
DT Article
DE Open ponds; Raceways; Light attenuation; Irradiance; Light spectra;
Photosynthesis
ID PHOTOSYNTHETIC ACTION; LIGHT-ABSORPTION; MICROALGAE; SPECTRA; BIOFUELS;
ENERGY; MICROORGANISMS; REGIMES; GROWTH
AB In this paper we report a method for experimental measurement of photosynthetic productivity as a function of simulated depth in open pond raceways for algae cultivation. Knowledge of the depth dependence of photosynthetic productivity aids in designing ponds with optimal depth with respect to biomass productivity and capital and operating costs. To simulate depth, we (i) measured irradiance attenuation coefficients of liquid algal cultures as a function of wavelength in the range of 400 to 700 nm, (ii) reproduced the magnitude and spectral content of the irradiance that would exist at various depths within open ponds using a programmable LED array, and (iii) measured photosynthetic rate as oxygen evolution under irradiances corresponding to various depths. We report the depth distribution of photosynthetic rate in simulated 20 cm deep ponds of the green alga Chlorella vulgaris and the cyanobacterium Spirulina platensis at a biomass concentration of 0.19 g dry biomass per liter (g/l). Under an incident irradiance corresponding to full sunlight, the compensation depth for Chlorella was 12 cm. Below this depth, net oxygen consumption due to respiration had a magnitude equal to 15% that of the total oxygen production above the compensation depth. For Spirulina, negative net oxygen production was not observed at any depth, but the top 13 cm of the pond accounted for 90% of its total oxygen production. These productivity cross-sections, in addition to knowledge of the dependence of capital and operating costs on pond depth, enable the design of open ponds for optimal depth for maximum return on investment. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Murphy, Thomas E.; Detweiler, Angela M.; Bebout, Brad M.; Prufert-Bebout, Leslie E.] NASA, Ames Res Ctr, Exobiol Dept, Moffett Field, CA 94035 USA.
[Kapili, Bennett J.] Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY 14850 USA.
RP Murphy, TE (reprint author), NASA, Ames Res Ctr, Mail Stop 239-4,POB 1, Moffett Field, CA 94035 USA.
EM thomasemurphy@utexas.edu
FU NASA Postdoctoral Program; NASA Internship Program; Cornell Tradition
Fellowship
FX The authors would like to thank Sue Carter at UC-Santa Cruz for the
lease of the TeleLumen LED array. The authors are also grateful for the
funding provided by the NASA Postdoctoral Program, the NASA Internship
Program, and the Cornell Tradition Fellowship. We would also like to
sincerely thank two anonymous reviewers, whose comments significantly
improved the manuscript.
NR 50
TC 2
Z9 2
U1 5
U2 24
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 2211-9264
J9 ALGAL RES
JI Algal Res.
PD SEP
PY 2015
VL 11
BP 334
EP 342
DI 10.1016/j.algal.2015.07.003
PG 9
WC Biotechnology & Applied Microbiology
SC Biotechnology & Applied Microbiology
GA CT8ED
UT WOS:000363046900040
ER
PT J
AU de Souza, RS
Cameron, E
Killedar, M
Hilbe, J
Vilalta, R
Maio, U
Biffi, V
Ciardi, B
Riggs, JD
AF de Souza, R. S.
Cameron, E.
Killedar, M.
Hilbe, J.
Vilalta, R.
Maio, U.
Biffi, V.
Ciardi, B.
Riggs, J. D.
CA COIN Collaboration
TI The overlooked potential of Generalized Linear Models in astronomy, I:
Binomial regression
SO ASTRONOMY AND COMPUTING
LA English
DT Article
DE Cosmology; First stars; Methods; Statistical; Stars; Population III
ID STAR-FORMATION; BAYESIAN-APPROACH; GALAXY CLUSTERS; MASS; SIMULATIONS;
REIONIZATION; ENVIRONMENT; SUPERNOVAE; EVOLUTION; DISTANCE
AB Revealing hidden patterns in astronomical data is often the path to fundamental scientific breakthroughs; meanwhile the complexity of scientific enquiry increases as more subtle relationships are sought. Contemporary data analysis problems often elude the capabilities of classical statistical techniques, suggesting the use of cutting edge statistical methods. In this light, astronomers have overlooked a whole family of statistical techniques for exploratory data analysis and robust regression, the so-called Generalized Linear Models (GLMs). In this paper - the first in a series aimed at illustrating the power of these methods in astronomical applications - we elucidate the potential of a particular class of GLMs for handling binary/binomial data, the so-called logit and probit regression techniques, from both a maximum likelihood and a Bayesian perspective. As a case in point, we present the use of these GLMs to explore the conditions of star formation activity and metal enrichment in primordial minihaloes from cosmological hydro-simulations including detailed chemistry, gas physics, and stellar feedback. We predict that for a dark mini-halo with metallicity approximate to 1.3 x 10(-4)Z(circle dot), an increase of 1.2 x 10(-2) in the gas molecular fraction, increases the probability of star formation occurrence by a factor of 75%. Finally, we highlight the use of receiver operating characteristic curves as a diagnostic for binary classifiers, and ultimately we use these to demonstrate the competitive predictive performance of GLMs against the popular technique of artificial neural networks. (C) 2015 Elsevier B.V. All rights reserved.
C1 [de Souza, R. S.] MTA Eotvos Univ, EIRSA Lendulet Astrophys Res Grp, H-1117 Budapest, Hungary.
[Cameron, E.] Univ Oxford, Dept Zool, Oxford OX1 3PS, England.
[Killedar, M.] Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Hilbe, J.] Arizona State Univ, Tempe, AZ 85287 USA.
[Hilbe, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Vilalta, R.] Univ Houston, Dept Comp Sci, Houston, TX 77204 USA.
[Maio, U.] Osserv Astron Trieste, INAF, I-34135 Trieste, Italy.
[Maio, U.] Leibniz Inst Astrophys, D-14482 Potsdam, Germany.
[Biffi, V.] SISSA, I-34136 Trieste, Italy.
[Ciardi, B.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Riggs, J. D.] Northwestern Univ, Evanston, IL 60208 USA.
RP de Souza, RS (reprint author), MTA Eotvos Univ, EIRSA Lendulet Astrophys Res Grp, H-1117 Budapest, Hungary.
EM rafael.2706@gmail.com; dr.ewan.cameron@gmail.com
RI Ciardi, Benedetta/N-7625-2015; de Souza, Rafael/C-8615-2013;
OI de Souza, Rafael/0000-0001-7207-4584; Maio, Umberto/0000-0002-0039-3102;
Hilbe, Joseph/0000-0002-4626-7961
FU DFG [DO 1310/4-1]; European Union [267251]
FX We thank the referee for very useful comments that helped to improve
this manuscript. We thank M. L. L. Dantas for the careful review and
fruitful comments of the manuscript. MK acknowledges support by the DFG
project DO 1310/4-1. UM would like to thank funding from a Marie Curie
Fellowship of the European Union Seventh Framework Project
(FP7/2007-2013), grant agreement n. 267251. Work on this paper has
substantially benefited from using the collaborative website AWOB
(http://awob.mpg.de) developed and maintained by the Max-Planck
Institute for Astrophysics and the Max-Planck Digital Library. The
bibliographic research was possible thanks to the tools offered by the
NASA Astrophysical Data Systems and the JSTOR archive.
NR 72
TC 7
Z9 7
U1 1
U2 3
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 2213-1337
EI 2213-1345
J9 ASTRON COMPUT
JI Astron. Comput.
PD SEP
PY 2015
VL 12
BP 21
EP 32
DI 10.1016/j.ascom.2015.04.002
PG 12
WC Astronomy & Astrophysics; Computer Science, Interdisciplinary
Applications
SC Astronomy & Astrophysics; Computer Science
GA CT5ON
UT WOS:000362859800003
ER
PT J
AU Indo, HP
Tomiyoshi, T
Suenaga, S
Tomita, K
Suzuki, H
Masuda, D
Terada, M
Ishioka, N
Gusev, O
Cornette, R
Okuda, T
Mukai, C
Majima, HJ
AF Indo, Hiroko P.
Tomiyoshi, Tsukasa
Suenaga, Shigeaki
Tomita, Kazuo
Suzuki, Hiromi
Masuda, Daisuke
Terada, Masahiro
Ishioka, Noriaki
Gusev, Oleg
Cornette, Richard
Okuda, Takashi
Mukai, Chiaki
Majima, Hideyuki J.
TI MnSOD downregulation induced by extremely low 0.1 mGy single and
fractionated X-rays and microgravity treatment in human neuroblastoma
cell line, NB-1
SO JOURNAL OF CLINICAL BIOCHEMISTRY AND NUTRITION
LA English
DT Article
DE space radiation; microgravity; extremely small dose; neuron; NB-1
ID IONIZING-RADIATION; SPACE RADIATION; GENE-EXPRESSION; DNA-DAMAGE;
HUMAN-LYMPHOCYTES; OXIDATIVE STRESS; DEATH; P53; SPACEFLIGHT; INDUCTION
AB A human neuroblastoma cell line, NB-1, was treated with 24 h of microgravity simulation by clinostat, or irradiated with extremely small X-ray doses of 0.1 or 1.0 mGy using single and 10 times fractionation regimes with 1 and 2 h time-intervals. A quantitative real-time reverse transcription polymerase chain reaction (qRT-PCR) examination was performed for apoptosis related factors (BAX, CYTC, APAF1, VDAC1-3, CASP3, CASP8, CASP9 P53, AIF, ANT1 and 2, BCL2, MnSOD, autophagy related BECN and necrosis related CYP-40. The qRT-PCR results revealed that microgravity did not result in significant changes except for a upregulation of proapoptotic VDAC2, and downregulations of proapoptotic CASP9 and antiapoptotic MnSOD. After 0.1 mGy fractionation irradiation, there was increased expression of proapoptotic APAF1 and downregulation of proapoptotic CYTC, VDAC2, VDAC3, CASP8, AIF, ANTI, and ANT2, as well as an increase in expression of antiapoptotic BCL2. There was also a decrease in MnSOD expression with 0.1 mGy fractionation irradiation. These results suggest that microgravity and low-dose radiation may decrease apoptosis but may potentially increase oxidative stress.
C1 [Indo, Hiroko P.; Tomiyoshi, Tsukasa; Suenaga, Shigeaki; Tomita, Kazuo; Majima, Hideyuki J.] Kagoshima Univ, Grad Sch Med & Dent Sci, Dept Oncol, Kagoshima 8908544, Japan.
[Suzuki, Hiromi; Masuda, Daisuke; Terada, Masahiro; Ishioka, Noriaki; Gusev, Oleg; Majima, Hideyuki J.] Kagoshima Univ, Grad Sch Med & Dent Sci, Dept Space Environm Med, Kagoshima 8908544, Japan.
[Suzuki, Hiromi] Japan Space Forum, Dept Sci & Applicat, Life Sci Res Grp, Tokyo 1000004, Japan.
[Masuda, Daisuke] Japan Manned Space Syst Corp, Utilizat & Engn Dept, Tsukuba, Ibaraki 3050047, Japan.
[Terada, Masahiro] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
[Ishioka, Noriaki; Gusev, Oleg] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Dept Space Biol & Micrograv Sci, Tsukuba, Ibaraki 3058505, Japan.
[Mukai, Chiaki] Japan Aerosp Explorat Agcy, Ctr Appl Space Med & Human Res, Tsukuba, Ibaraki 3058505, Japan.
[Gusev, Oleg] Kazan Fed Univ, Inst Fundamental Med & Biol, Dept Invertebrates Zool & Funct Morphol, Kazan 420008, Russia.
[Gusev, Oleg; Cornette, Richard; Okuda, Takashi] Natl Inst Agrobiol Sci, Anhydrobiosis Res Unit, Tsukuba, Ibaraki 3058634, Japan.
RP Majima, HJ (reprint author), Kagoshima Univ, Grad Sch Med & Dent Sci, Dept Oncol, 8-35-1 Sakuragaoka, Kagoshima 8908544, Japan.
EM hmajima@dent.kagoshima-u.ac.jp
RI Gusev, Oleg/D-9383-2011
OI Gusev, Oleg/0000-0002-6203-9758
FU Strategic Promotion Program for Basic Nuclear Research of the Ministry
of Education, Culture, Sports, Science and Technology of Japan; Program
for Promotion of Basic and Applied Researches for Innovations in
Bio-oriented Industry (BRAIN) by the Ministry of Agriculture, Forestry
and Fisheries of Japan; [22592093]; [23592774]
FX The authors would like to express their appreciation to Dr. Aaron K.
Holley for the helpful discussion. This work was supported in part by a
Grant-in-Aid for Scientific Research (C) (No. 22592093 to H.J.M. and No.
23592774 to H.P.I.) and the Strategic Promotion Program for Basic
Nuclear Research (to H.J.M.) of the Ministry of Education, Culture,
Sports, Science and Technology of Japan; and the Program for Promotion
of Basic and Applied Researches for Innovations in Bio-oriented Industry
(BRAIN) (to H.J.M.) by the Ministry of Agriculture, Forestry and
Fisheries of Japan.
NR 57
TC 5
Z9 5
U1 1
U2 3
PU JOURNAL CLINICAL BIOCHEMISTRY & NUTRITION
PI KYOTO
PA KYOTO PREFECTURAL UNIV MED, GRAD SCH MEDICAL SCIENCE, DEPT MOLECULAR
GASTROENTEROLOGY & HEPATOLOGY, KYOTO, 602-8566, JAPAN
SN 0912-0009
EI 1880-5086
J9 J CLIN BIOCHEM NUTR
JI J. Clin. Biochem. Nutr.
PD SEP 1
PY 2015
VL 57
IS 2
BP 98
EP 104
DI 10.3164/jcbn.15-20
PG 7
WC Nutrition & Dietetics
SC Nutrition & Dietetics
GA CT2JL
UT WOS:000362627700002
PM 26388666
ER
PT J
AU Boujibar, A
Andrault, D
Bolfan-Casanova, N
Bouhifd, MA
Monteux, J
AF Boujibar, Asmaa
Andrault, Denis
Bolfan-Casanova, Nathalie
Bouhifd, Mohamed Ali
Monteux, Julien
TI Cosmochemical fractionation by collisional erosion during the Earth's
accretion
SO NATURE COMMUNICATIONS
LA English
DT Article
ID NON-CHONDRITIC COMPOSITION; SOLAR-SYSTEM; TERRESTRIAL PLANETS; CHONDRULE
FORMATION; PHASE-RELATIONS; CORE FORMATION; HIGH-PRESSURE; POTASSIUM;
ORIGIN; IMPACT
AB Early in the Solar System's history, energetic collisions of differentiated bodies affected the final composition of the terrestrial planets through partial destruction. Enstatite chondrites (EC) are the best candidates to represent the primordial terrestrial precursors as they present the most similar isotopic compositions to Earth. Here we report that collisional erosion of >15% of the early Earth's mass can reconcile the remaining compositional differences between EC and the Earth. We base our demonstration on experimental melting of an EC composition at pressures between 1 bar and 25 GPa. At low pressures, the first silicate melts are highly enriched in incompatible elements Si, Al and Na, and depleted in Mg. Loss of proto-crusts through impacts raises the Earth's Mg/Si ratio to its present value. To match all major element compositions, our model implies preferential loss of volatile lithophile elements and re-condensation of refractory lithophile elements after the impacts.
C1 [Boujibar, Asmaa; Andrault, Denis; Bolfan-Casanova, Nathalie; Bouhifd, Mohamed Ali; Monteux, Julien] Univ Clermont Ferrand, Lab Magmas & Volcans, CNRS, UMR 6524, F-63000 Clermont Ferrand, France.
RP Boujibar, A (reprint author), NASA, Johnson Space Ctr, Astromat Res & Explorat Sci, 2101 Nasa Pkwy, Houston, TX 77058 USA.
EM asmaa.boujibar@nasa.gov
RI Boujibar, Asmaa/D-7270-2014; ANDRAULT, Denis/N-8843-2016
OI Boujibar, Asmaa/0000-0002-9036-4726; ANDRAULT, Denis/0000-0002-9921-4572
FU INSU-CNRS; ANR 'Oxydeep' project; Universite Blaise Pascal; Region
Auvergne
FX We thank B. Bourdon, M. Boyet, S. Charnoz, M. Javoy, E. Kaminski, R.
Mishra, S. Keshav, D. Laporte, G. Libourel, H. Martin, Y. Marrocchi, M.
Toplis, K. Righter and M. Zolensky for their fruitful discussions and
various members of the Laboratoire Magmas et Volcans staff for essential
help. This project received funds from INSU-CNRS, Universite Blaise
Pascal, Region Auvergne and the ANR 'Oxydeep' project. It is a LabEx
Clervolc 170 contribution.
NR 44
TC 3
Z9 3
U1 2
U2 17
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD SEP
PY 2015
VL 6
AR 8295
DI 10.1038/ncomms9295
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CT7UJ
UT WOS:000363019700002
PM 26395157
ER
PT J
AU Fletcher, A
Close, S
Mathias, D
AF Fletcher, Alex
Close, Sigrid
Mathias, Donovan
TI Simulating plasma production from hypervelocity impacts
SO PHYSICS OF PLASMAS
LA English
DT Article
ID SMOOTHED PARTICLE HYDRODYNAMICS; GENERATED PLASMA; SPH; EMISSIONS;
METEOROIDS; SPACECRAFT; DEBRIS; CODE
AB Hypervelocity particles, such as meteoroids and space debris, routinely impact spacecraft and are energetic enough to vaporize and ionize themselves and as well as a portion of the target material. The resulting plasma rapidly expands into the surrounding vacuum. While plasma measurements from hypervelocity impacts have been made using ground-based technologies such as light gas guns and Van de Graaff dust accelerators, some of the basic plasma properties vary significantly between experiments. There have been both ground-based and in-situ measurements of radio frequency (RF) emission from hypervelocity impacts, but the physical mechanism responsible and the possible connection to the impact-produced plasma are not well understood. Under certain conditions, the impact-produced plasma can have deleterious effects on spacecraft electronics by providing a new current path, triggering an electrostatic discharge, causing electromagnetic interference, or generating an electromagnetic pulse. Multi-physics simulations of plasma production from hypervelocity impacts are presented. These simulations incorporate elasticity and plasticity of the solid target, phase change and plasma formation, and non-ideal plasma physics due to the high density and low temperature of the plasma. A smoothed particle hydrodynamics method is used to perform a continuum dynamics simulation with these additional physics. By examining a series of hypervelocity impacts, basic properties of the impact produced plasma plume (density, temperature, expansion speed, charge state) are determined for impactor speeds between 10 and 72 km/s. For a large range of higher impact speeds (30-72 km/s), we find the temperature is unvarying at 2.5 eV. We also find that the plasma plume is weakly ionized for impact speeds less than 14 km/s and fully ionized for impact speeds greater than 20 km/s, independent of impactor mass. This is the same velocity threshold for the detection of RF emission in recent Van de Graaff experiments, suggesting that the RF is correlated to the formation of fully ionized plasma. (C) 2015 AIP Publishing LLC.
C1 [Fletcher, Alex; Close, Sigrid] Stanford Univ, Aeronaut & Astronaut, Stanford, CA 94305 USA.
[Mathias, Donovan] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Fletcher, A (reprint author), Stanford Univ, Aeronaut & Astronaut, 496 Lomita Mall, Stanford, CA 94305 USA.
EM alexcf@stanford.edu
FU Department of Energy [DE-SC0010390]; Air Force Office of Scientific
Research Grant [FA9550-14-1-0290 DEF]; Engineering Risk Assessment team
at NASA Ames Research Center
FX This work was supported by Department of Energy Grant No. DE-SC0010390,
Air Force Office of Scientific Research Grant No. FA9550-14-1-0290 DEF,
and the Engineering Risk Assessment team at NASA Ames Research Center.
NR 48
TC 3
Z9 3
U1 3
U2 12
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 SEP
PY 2015
VL 22
IS 9
AR 093504
DI 10.1063/1.4930281
PG 11
WC Physics, Fluids & Plasmas
SC Physics
GA CT1PM
UT WOS:000362571800117
ER
PT J
AU Lopez, RA
Munoz, V
Vinas, AF
Valdivia, JA
AF Lopez, Rodrigo A.
Munoz, Victor
Vinas, Adolfo F.
Valdivia, Juan A.
TI Propagation of localized structures in relativistic magnetized
electron-positron plasmas using particle-in-cell simulations
SO PHYSICS OF PLASMAS
LA English
DT Article
ID ALFVENIC WAVE-PACKETS; HOT ACCRETION DISKS; PAIR PLASMAS; GAUSS LAW;
CODES; GENERATION
AB We use a particle-in-cell simulation to study the propagation of localized structures in a magnetized electron-positron plasma with relativistic finite temperature. We use as initial condition for the simulation an envelope soliton solution of the nonlinear Schrodinger equation, derived from the relativistic two fluid equations in the strongly magnetized limit. This envelope soliton turns out not to be a stable solution for the simulation and splits in two localized structures propagating in opposite directions. However, these two localized structures exhibit a soliton-like behavior, as they keep their profile after they collide with each other due to the periodic boundary conditions. We also observe the formation of localized structures in the evolution of a spatially uniform circularly polarized Alfven wave. In both cases, the localized structures propagate with an amplitude independent velocity. (C) 2015 AIP Publishing LLC.
C1 [Lopez, Rodrigo A.] Univ Concepcion, Dept Fis, Fac Ciencias Fis & Matemat, Concepcion 4070386, Chile.
[Munoz, Victor; Valdivia, Juan A.] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile.
[Vinas, Adolfo F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Valdivia, Juan A.] Ctr Desarrollo Nanociencia & Nanotecnol CEDENNA, Santiago 9170124, Chile.
RP Lopez, RA (reprint author), Univ Concepcion, Dept Fis, Fac Ciencias Fis & Matemat, Concepcion 4070386, Chile.
RI Lopez, Rodrigo/H-7576-2013; Valdivia, Juan/A-3631-2008; Munoz,
Victor/A-2255-2008
OI Valdivia, Juan/0000-0003-3381-9904;
FU CONICyT through FONDECyT [1150718, 1130273, 1121144, 3140142]; CEDENNA;
NASA-Wind/SWE project
FX We thank the support of CONICyT through FONDECyT Grants Nos. 1150718 and
1130273 (J.A.V.); No. 1121144 (V.M.); and Postdoctoral Grant No.
3140142. (R.A.L.). We also thank financial support from CEDENNA. A.F.V.
would like to thank the NASA-Wind/SWE project for their support.
NR 47
TC 1
Z9 1
U1 1
U2 6
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 SEP
PY 2015
VL 22
IS 9
AR 092115
DI 10.1063/1.4930266
PG 7
WC Physics, Fluids & Plasmas
SC Physics
GA CT1PM
UT WOS:000362571800030
ER
PT J
AU Hofmann, DC
Hamill, L
Christiansen, E
Nutt, S
AF Hofmann, Douglas C.
Hamill, Lee
Christiansen, Eric
Nutt, Steve
TI Hypervelocity Impact Testing of a Metallic Glass-Stuffed Whipple Shield
SO ADVANCED ENGINEERING MATERIALS
LA English
DT Article
ID MATRIX COMPOSITES; ORBITAL DEBRIS; SPACECRAFT; HONEYCOMB
AB In this work, hypervelocity impact tests up to 7 km.s(-1) are used to compare the performance of Whipple shields integrated with layers of metallic glasses with a baseline target analogue of one of the shields similar to what is used on the International Space Station. The baseline target failed under the impact while the target utilizing metallic glass as a replacement for the fabric layers in the baseline passed the test. The paper postulates on the prospects of future implementation of metallic glasses as spacecraft debris shields.
C1 [Hofmann, Douglas C.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Hofmann, Douglas C.] CALTECH, Keck Lab Engn Sci, Pasadena, CA 91125 USA.
[Hamill, Lee; Nutt, Steve] Univ So Calif, Los Angeles, CA USA.
[Christiansen, Eric] NASA, Johnson Space Ctr, Houston, TX USA.
RP Hofmann, DC (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM dch@jpl.nasa.gov
FU Office of Air Force Research [FA9550-12-1-0059_5]; NASA's Exploration
Systems Mission Directorate [MSFC-NRA10]
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. This work was funded by the Office
of Air Force Research under grant number FA9550-12-1-0059_5 and NASA's
Exploration Systems Mission Directorate under Contract No. MSFC-NRA10.
The authors thank the staff of the White Sands Test Facility for their
assistance with the tests and A. Kunz for sample preparation.
NR 23
TC 2
Z9 2
U1 5
U2 22
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA POSTFACH 101161, 69451 WEINHEIM, GERMANY
SN 1438-1656
EI 1527-2648
J9 ADV ENG MATER
JI Adv. Eng. Mater.
PD SEP
PY 2015
VL 17
IS 9
BP 1313
EP 1322
DI 10.1002/adem.201400518
PG 10
WC Materials Science, Multidisciplinary
SC Materials Science
GA CT0VM
UT WOS:000362515600009
ER
PT J
AU Cockrell, AL
Fitzgerald, LA
Cusick, KD
Barlow, DE
Tsoi, SD
Soto, CM
Baldwin, JW
Dale, JR
Morris, RE
Little, BJ
Biffinger, JC
AF Cockrell, Allison L.
Fitzgerald, Lisa A.
Cusick, Kathleen D.
Barlow, Daniel E.
Tsoi, Stanislav D.
Soto, Carissa M.
Baldwin, Jeffrey W.
Dale, Jason R.
Morris, Robert E.
Little, Brenda J.
Biffinger, Justin C.
TI Differences in Physical and Biochemical Properties of Thermus
scotoductus SA-01 Cultured with Dielectric or Convection Heating
SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY
LA English
DT Article
ID BACTERIAL-CELL; SPECTROSCOPY; MICROORGANISMS; IDENTIFICATION;
MICROBIOLOGY; IRRADIATION; MICROSCOPY; PRESSURE; LIFE
AB A thermophile, Thermus scotoductus SA-01, was cultured within a constant-temperature (65 degrees C) microwave (MW) digester to determine if MW-specific effects influenced the growth and physiology of the organism. As a control, T. scotoductus cells were also cultured using convection heating at the same temperature as the MW studies. Cell growth was analyzed by optical density (OD) measurements, and cell morphologies were characterized using electron microscopy imaging (scanning electron microscopy [SEM] and transmission electron microscopy [TEM]), dynamic light scattering (DLS), and atomic force microscopy (AFM). Biophysical properties (i.e., turgor pressure) were also calculated with AFM, and biochemical compositions (i.e., proteins, nucleic acids, fatty acids) were analyzed by attenuated total reflectance-Fourier transform infrared (ATR-FTIR) spectroscopy. Gas chromatography-mass spectrometry (GC-MS) was used to analyze the fatty acid methyl esters extracted from cell membranes. Here we report successful cultivation of a thermophile with only dielectric heating. Under the MW conditions for growth, cell walls remained intact and there were no indications of membrane damage or cell leakage. Results from these studies also demonstrated that T. scotoductus cells grown with MW heating exhibited accelerated growth rates in addition to altered cell morphologies and biochemical compositions compared with oven-grown cells.
C1 [Cockrell, Allison L.; Fitzgerald, Lisa A.; Cusick, Kathleen D.; Barlow, Daniel E.; Tsoi, Stanislav D.; Morris, Robert E.; Biffinger, Justin C.] US Naval Res Lab, Div Chem, Washington, DC 20375 USA.
[Soto, Carissa M.] US Naval Res Lab, Ctr Biomol Sci & Engn, Washington, DC USA.
[Baldwin, Jeffrey W.] US Naval Res Lab, Acoust Div, Washington, DC USA.
[Dale, Jason R.; Little, Brenda J.] US Naval Res Lab, Geosci Div, Stennis Space Ctr, Washington, DC USA.
RP Biffinger, JC (reprint author), US Naval Res Lab, Div Chem, Washington, DC 20375 USA.
EM Justin.biffinger@nrl.navy.mil
FU ONR/NRL Blk 6.1 Nanoscience Institute; National Research Council
FX This work was funded by ONR/NRL Blk 6.1 Nanoscience Institute funding.
We thank the National Research Council for A.L.C.'s and K.D.C.'s
postdoctoral research associateships.
NR 41
TC 1
Z9 1
U1 4
U2 7
PU AMER SOC MICROBIOLOGY
PI WASHINGTON
PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA
SN 0099-2240
EI 1098-5336
J9 APPL ENVIRON MICROB
JI Appl. Environ. Microbiol.
PD SEP
PY 2015
VL 81
IS 18
BP 6285
EP 6293
DI 10.1128/AEM.01618-15
PG 9
WC Biotechnology & Applied Microbiology; Microbiology
SC Biotechnology & Applied Microbiology; Microbiology
GA CT2ZU
UT WOS:000362676400019
PM 26150459
ER
PT J
AU Ade, PAR
Aghanim, N
Armitage-Caplan, C
Arnaud, M
Ashdown, M
Atrio-Barandela, F
Aumont, J
Aussel, H
Baccigalupi, C
Banday, AJ
Barreiro, RB
Barrena, R
Bartelmann, M
Bartlett, JG
Battaner, E
Benabed, K
Benoit, A
Benoit-Levy, A
Bernard, JP
Bersanelli, M
Bielewicz, P
Bikmaev, I
Bobin, J
Bock, JJ
Bohringer, H
Bonaldi, A
Bond, JR
Borrill, J
Bouchet, FR
Bridges, M
Bucher, M
Burenin, R
Burigana, C
Butler, RC
Cardoso, JF
Carvalho, P
Catalano, A
Challinor, A
Chamballu, A
Chary, RR
Chen, X
Chiang, HC
Chiang, LY
Chon, G
Christensen, PR
Churazov, E
Church, S
Clements, DL
Colombi, S
Colombo, LPL
Comis, B
Couchot, F
Coulais, A
Crill, BP
Curto, A
Cuttaia, F
Da Silva, A
Dahle, H
Danese, L
Davies, RD
Davis, RJ
de Bernardis, P
de Rosa, A
de Zotti, G
Delabrouille, J
Delouis, JM
Democles, J
Desert, FX
Dickinson, C
Diego, JM
Dolag, K
Dole, H
Donzelli, S
Dore, O
Douspis, M
Dupac, X
Efstathiou, G
Ensslin, TA
Eriksen, HK
Feroz, F
Ferragamo, A
Finelli, F
Flores-Cacho, I
Forni, O
Frailis, M
Franceschi, E
Fromenteau, S
Galeotta, S
Ganga, K
Genova-Santos, RT
Giard, M
Giardino, G
Gilfanov, M
Giraud-Heraud, Y
Gonzalez-Nuevo, J
Gorski, KM
Grainge, KJB
Gratton, S
Gregorio, A
Groeneboom, NE
Gruppuso, A
Hansen, FK
Hanson, D
Harrison, D
Hempel, A
Henrot-Versille, S
Hernandez-Monteagudo, C
Herranz, D
Hildebrandt, SR
Hivon, E
Hobson, M
Holmes, WA
Hornstrup, A
Hovest, W
Huffenberger, KM
Hurier, G
Hurley-Walker, N
Jaffe, AH
Jaffe, TR
Jones, WC
Juvela, M
Keihanen, E
Keskitalo, R
Khamitov, I
Kisner, TS
Kneissl, R
Knoche, J
Knox, L
Kunz, M
Kurki-Suonio, H
Lagache, G
Lahteenmaki, A
Lamarre, JM
Lasenby, A
Laureijs, RJ
Lawrence, CR
Leahy, JP
Leonardi, R
Leon-Tavares, J
Lesgourgues, J
Li, C
Liddle, A
Liguori, M
Lilje, PB
Linden-Vornle, M
Lopez-Caniego, M
Lubin, PM
Macias-Perez, JF
MacTavish, CJ
Maffei, B
Maino, D
Mandolesi, N
Maris, M
Marshall, DJ
Martin, PG
Martinez-Gonzalez, E
Masi, S
Massardi, M
Matarrese, S
Matthai, F
Mazzotta, P
Mei, S
Meinhold, PR
Melchiorri, A
Melin, JB
Mendes, L
Mennella, A
Migliaccio, M
Mikkelsen, K
Mitra, S
Miville-Deschenes, MA
Moneti, A
Montier, L
Morgante, G
Mortlock, D
Munshi, D
Murphy, JA
Naselsky, P
Nastasi, A
Nati, F
Natoli, P
Nesvadba, NPH
Netterfield, CB
Norgaard-Nielsen, HU
Noviello, F
Novikov, D
Novikov, I
O'Dwyer, IJ
Olamaie, M
Osborne, S
Oxborrow, CA
Paci, F
Pagano, L
Pajot, F
Paoletti, D
Pasian, F
Patanchon, G
Pearson, TJ
Perdereau, O
Perotto, L
Perrott, YC
Perrotta, F
Piacentini, F
Piat, M
Pierpaoli, E
Pietrobon, D
Plaszczynski, S
Pointecouteau, E
Polenta, G
Ponthieu, N
Popa, L
Poutanen, T
Pratt, GW
Prezeau, G
Prunet, S
Puget, JL
Rachen, JP
Reach, WT
Rebolo, R
Reinecke, M
Remazeilles, M
Renault, C
Ricciardi, S
Riller, T
Ristorcellinon, I
Rocha, G
Rossee, C
Roudier, G
Rowan-Robinson, M
Rubino-Martin, JA
Rumsey, C
Rusholme, B
Sandri, M
Santos, D
Saunders, RDE
Savini, G
Schammer, MP
Scott, D
Seiffert, MD
Shellard, EPS
Shimwele, TW
Spencer, LD
Starck, JL
Stolyarov, V
Stompor, R
Streblyanska, A
Sudiwala, R
Sunyaev, R
Sureau, F
Sutton, D
Suur-Uski, AS
Sygnet, JF
Tauber, JA
Tavagnacco, D
Terenzi, L
Toffolatti, L
Tomasi, M
Tramonte, D
Tristram, M
Tucci, M
Tuovinee, J
Turler, M
Umana, G
Valenziano, L
Valiviita, J
Van Tent, B
Vibert, L
Vielva, P
Villa, F
Vittorio, N
Wade, LA
Wandelt, BD
White, M
White, SDM
Yvon, D
Zacchei, A
Zonca, A
AF Ade, P. A. R.
Aghanim, N.
Armitage-Caplan, C.
Arnaud, M.
Ashdown, M.
Atrio-Barandela, F.
Aumont, J.
Aussel, H.
Baccigalupi, C.
Banday, A. J.
Barreiro, R. B.
Barrena, R.
Bartelmann, M.
Bartlett, J. G.
Battaner, E.
Benabed, K.
Benoit, A.
Benoit-Levy, A.
Bernard, J. -P.
Bersanelli, M.
Bielewicz, P.
Bikmaev, I.
Bobin, J.
Bock, J. J.
Boehringer, H.
Bonaldi, A.
Bond, J. R.
Borrill, J.
Bouchet, F. R.
Bridges, M.
Bucher, M.
Burenin, R.
Burigana, C.
Butler, R. C.
Cardoso, J. -F.
Carvalho, P.
Catalano, A.
Challinor, A.
Chamballu, A.
Chary, R. -R.
Chen, X.
Chiang, H. C.
Chiang, L. -Y
Chon, G.
Christensen, P. R.
Churazov, E.
Church, S.
Clements, D. L.
Colombi, S.
Colombo, L. P. L.
Comis, B.
Couchot, F.
Coulais, A.
Crill, B. P.
Curto, A.
Cuttaia, F.
Da Silva, A.
Dahle, H.
Danese, L.
Davies, R. D.
Davis, R. J.
de Bernardis, P.
de Rosa, A.
de Zotti, G.
Delabrouille, J.
Delouis, J. -M.
Democles, J.
Desert, F. -X.
Dickinson, C.
Diego, J. M.
Dolag, K.
Dole, H.
Donzelli, S.
Dore, O.
Douspis, M.
Dupac, X.
Efstathiou, G.
Ensslin, T. A.
Eriksen, H. K.
Feroz, F.
Ferragamo, A.
Finelli, F.
Flores-Cacho, I.
Forni, O.
Frailis, M.
Franceschi, E.
Fromenteau, S.
Galeotta, S.
Ganga, K.
Genova-Santos, R. T.
Giard, M.
Giardino, G.
Gilfanov, M.
Giraud-Heraud, Y.
Gonzalez-Nuevo, J.
Gorski, K. M.
Grainge, K. J. B.
Gratton, S.
Gregorio, A.
Groeneboom, N. E.
Gruppuso, A.
Hansen, F. K.
Hanson, D.
Harrison, D.
Hempel, A.
Henrot-Versille, S.
Hernandez-Monteagudo, C.
Herranz, D.
Hildebrandt, S. R.
Hivon, E.
Hobson, M.
Holmes, W. A.
Hornstrup, A.
Hovest, W.
Huffenberger, K. M.
Hurier, G.
Hurley-Walker, N.
Jaffe, A. H.
Jaffe, T. R.
Jones, W. C.
Juvela, M.
Keihanen, E.
Keskitalo, R.
Khamitov, I.
Kisner, T. S.
Kneissl, R.
Knoche, J.
Knox, L.
Kunz, M.
Kurki-Suonio, H.
Lagache, G.
Lahteenmaki, A.
Lamarre, J. -M.
Lasenby, A.
Laureijs, R. J.
Lawrence, C. R.
Leahy, J. P.
Leonardi, R.
Leon-Tavares, J.
Lesgourgues, J.
Li, C.
Liddle, A.
Liguori, M.
Lilje, P. B.
Linden-Vornle, M.
Lopez-Caniego, M.
Lubin, P. M.
Macias-Perez, J. F.
MacTavish, C. J.
Maffei, B.
Maino, D.
Mandolesi, N.
Maris, M.
Marshall, D. J.
Martin, P. G.
Martinez-Gonzalez, E.
Masi, S.
Massardi, M.
Matarrese, S.
Matthai, F.
Mazzotta, P.
Mei, S.
Meinhold, P. R.
Melchiorri, A.
Melin, J. -B.
Mendes, L.
Mennella, A.
Migliaccio, M.
Mikkelsen, K.
Mitra, S.
Miville-Deschenes, M. -A.
Moneti, A.
Montier, L.
Morgante, G.
Mortlock, D.
Munshi, D.
Murphy, J. A.
Naselsky, P.
Nastasi, A.
Nati, F.
Natoli, P.
Nesvadba, N. P. H.
Netterfield, C. B.
Norgaard-Nielsen, H. U.
Noviello, F.
Novikov, D.
Novikov, I.
O'Dwyer, I. J.
Olamaie, M.
Osborne, S.
Oxborrow, C. A.
Paci, F.
Pagano, L.
Pajot, F.
Paoletti, D.
Pasian, F.
Patanchon, G.
Pearson, T. J.
Perdereau, O.
Perotto, L.
Perrott, Y. C.
Perrotta, F.
Piacentini, F.
Piat, M.
Pierpaoli, E.
Pietrobon, D.
Plaszczynski, S.
Pointecouteau, E.
Polenta, G.
Ponthieu, N.
Popa, L.
Poutanen, T.
Pratt, G. W.
Prezeau, G.
Prunet, S.
Puget, J. -L.
Rachen, J. P.
Reach, W. T.
Rebolo, R.
Reinecke, M.
Remazeilles, M.
Renault, C.
Ricciardi, S.
Riller, T.
Ristorcellinon, I.
Rocha, G.
Rossee, C.
Roudier, G.
Rowan-Robinson, M.
Rubino-Martin, J. A.
Rumsey, C.
Rusholme, B.
Sandri, M.
Santos, D.
Saunders, R. D. E.
Savini, G.
Schammer, M. P.
Scott, D.
Seiffert, M. D.
Shellard, E. P. S.
Shimwele, T. W.
Spencer, L. D.
Starck, J. -L.
Stolyarov, V.
Stompor, R.
Streblyanska, A.
Sudiwala, R.
Sunyaev, R.
Sureau, F.
Sutton, D.
Suur-Uski, A. -S.
Sygnet, J. -F.
Tauber, J. A.
Tavagnacco, D.
Terenzi, L.
Toffolatti, L.
Tomasi, M.
Tramonte, D.
Tristram, M.
Tucci, M.
Tuovinee, J.
Turler, M.
Umana, G.
Valenziano, L.
Valiviita, J.
Van Tent, B.
Vibert, L.
Vielva, P.
Villa, F.
Vittorio, N.
Wade, L. A.
Wandelt, B. D.
White, M.
White, S. D. M.
Yvon, D.
Zacchei, A.
Zonca, A.
CA Planck Collaboration
TI Planck 2013 results. XXXII. The updated Planck catalogue of
Sunyaev-Zeldovich sources
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE errata, addenda; large-scale structure of Universe; galaxies: clusters:
general; catalogs
ID GALAXY CLUSTERS; PAN-STARRS; TELESCOPE
AB We update the all-sky Planck catalogue of 1227 clusters and cluster candidates (PSZ1) published in March 2013, derived from detections of the Sunyaev-Zeldovich (SZ) effect using the first 15.5 months of Planck satellite observations. As an addendum, we deliver an updated version of the PSZ1 catalogue, reporting the further confirmation of 86 Planck-discovered clusters. In total, the PSZ1 now contains 947 confirmed clusters, of which 214 were confirmed as newly discovered clusters through follow-up observations undertaken by the Planck Collaboration. The updated PSZ1 contains redshifts for 913 systems, of which 736 (similar to 80.6%) are spectroscopic, and associated mass estimates derived from the Y-z mass proxy. We also provide a new SZ quality flag for the remaining 280 candidates. This flag was derived from a novel artificial neural-network classification of the SZ signal. Based on this assessment, the purity of the updated PSZ1 catalogue is estimated to be 94%. In this release, we provide the full updated catalogue and an additional readme file with further information on the Planck SZ detections.
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RP Aghanim, N (reprint author), Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France.
EM nabila.aghanim@ias.u-psud.fr
RI Butler, Reginald/N-4647-2015; Remazeilles, Mathieu/N-1793-2015; Novikov,
Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati,
Federico/I-4469-2016; popa, lucia/B-4718-2012; Vielva,
Patricio/F-6745-2014; Pearson, Timothy/N-2376-2015; Lopez-Caniego,
Marcos/M-4695-2013; Martinez-Gonzalez, Enrique/E-9534-2015; Piacentini,
Francesco/E-7234-2010; Gonzalez-Nuevo, Joaquin/I-3562-2014;
Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017;
Kurki-Suonio, Hannu/B-8502-2016; Gruppuso, Alessandro/N-5592-2015;
Toffolatti, Luigi/K-5070-2014; Lahteenmaki, Anne/L-5987-2013; Tomasi,
Maurizio/I-1234-2016; White, Martin/I-3880-2015; Herranz,
Diego/K-9143-2014; Novikov, Dmitry/P-1807-2015; Hurley-Walker,
Natasha/B-9520-2013; Valiviita, Jussi/A-9058-2016; Mazzotta,
Pasquale/B-1225-2016; Churazov, Eugene/A-7783-2013
OI Reach, William/0000-0001-8362-4094; Hurier,
Guillaume/0000-0002-1215-0706; Zacchei, Andrea/0000-0003-0396-1192;
Hivon, Eric/0000-0003-1880-2733; Butler, Reginald/0000-0003-4366-5996;
Huffenberger, Kevin/0000-0001-7109-0099; Burigana,
Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924;
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; Cuttaia, Francesco/0000-0001-6608-5017;
Remazeilles, Mathieu/0000-0001-9126-6266; Maris,
Michele/0000-0001-9442-2754; Galeotta, Samuele/0000-0002-3748-5115;
Pasian, Fabio/0000-0002-4869-3227; Scott, Douglas/0000-0002-6878-9840;
Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego,
Marcos/0000-0003-1016-9283; Polenta, Gianluca/0000-0003-4067-9196;
Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147;
Savini, Giorgio/0000-0003-4449-9416; Pierpaoli,
Elena/0000-0002-7957-8993; Morgante, Gianluca/0000-0001-9234-7412;
Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388;
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; Colombo,
Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Vielva,
Patricio/0000-0003-0051-272X; Pearson, Timothy/0000-0001-5213-6231;
Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Piacentini,
Francesco/0000-0002-5444-9327; Gonzalez-Nuevo,
Joaquin/0000-0003-1354-6822; Atrio-Barandela,
Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X;
Kurki-Suonio, Hannu/0000-0002-4618-3063; Gruppuso,
Alessandro/0000-0001-9272-5292; Toffolatti, Luigi/0000-0003-2645-7386;
Tomasi, Maurizio/0000-0002-1448-6131; White, Martin/0000-0001-9912-5070;
Herranz, Diego/0000-0003-4540-1417; Hurley-Walker,
Natasha/0000-0002-5119-4808; Valiviita, Jussi/0000-0001-6225-3693;
Mazzotta, Pasquale/0000-0002-5411-1748;
FU 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); CCI International Time Programme;
Alfred P. Sloan Foundation; National Science Foundation; DoE; NASA;
CNES; CNRS
FX 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). The authors thank N. Schartel, ESA
XMM-Newton project scientist, for granting the DDT used for confirmation
of SZ Planck candidates. The authors thank TUBITAK, IKI, KFU and AST for
support in using RTT150; in particular we thank KFU and IKI for
providing significant amounts of their observing time at RTT150. We also
acknowledge the BTA 6 m telescope TAC for support of the optical
follow-up project. The authors acknowledge the use of the INT and WHT
telescopes operated on the island of La Palma by the Isaac Newton Group
of Telescopes at the Spanish Observatorio del Roque de los Muchachos of
the IAC; the NOT, operated on La Palma jointly by Denmark, Finland,
Iceland, Norway, and Sweden, at the Spanish Observatorio del Roque de
los Muchachos; the TNG, operated on La Palma by the Fundacion Galileo
Galilei of the INAF at the Spanish Observatorio del Roque de los
Muchachos; the GTC telescope, operated on La Palma by the IAC at the
Spanish Observatorio del Roque de los Muchachos; and the IAC80 telescope
operated on the island of Tenerife by the IAC at the Spanish
Observatorio del Teide. Part of this research has been carried out with
telescope time awarded by the CCI International Time Programme. The
authors thank the TAC of the MPG/ESO-2.2m telescope for support of
optical follow-up with WFI under Max Planck time. Observations were also
conducted with ESO NTT at the La Silla Paranal Observatory. This
research has made use of SDSS-III data. Funding for SDSS-III
(http://www.sdss3.org/) has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, and DoE. SDSS-III is managed by the Astrophysical Research
Consortium for the Participating Institutions of the SDSS-III
Collaboration. This research has made use of the following databases:
the NED and IRSA databases, operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the NASA;
SIMBAD, operated at CDS, Strasbourg, France; SZ cluster database (http
://szcluster-db.ias.u-psud.fr) and SZ repository operated by IDOC
operated by IAS under contract with CNES and CNRS.
NR 16
TC 5
Z9 5
U1 3
U2 16
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2015
VL 581
AR A14
DI 10.1051/0004-6361/201525787
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1DX
UT WOS:000361803900014
ER
PT J
AU Bognar, Z
Lampens, P
Fremat, Y
Southworth, J
Sodor, A
De Cat, P
Isaacson, HT
Marcy, GW
Ciardi, DR
Gilliland, RL
Martin-Fernandez, P
AF Bognar, Zs
Lampens, P.
Fremat, Y.
Southworth, J.
Sodor, A.
De Cat, P.
Isaacson, H. T.
Marcy, G. W.
Ciardi, D. R.
Gilliland, R. L.
Martin-Fernandez, P.
TI KIC 9533489: a genuine gamma Doradus - delta Scuti Kepler hybrid
pulsator with transit events
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: photometric; stars: individual: KIC 9533489; stars:
variables: delta Scuti; planets and satellites: detection; stars:
oscillations
ID LONG-CADENCE DATA; ORDER G-MODES; INITIAL CHARACTERISTICS; STELLAR
OSCILLATIONS; EXTRASOLAR PLANETS; MAIN-SEQUENCE; STARS;
ASTEROSEISMOLOGY; TELESCOPE; ROTATION
AB Context. Several hundred candidate hybrid pulsators of type A-F have been identified from space-based observations. Their large number allows both statistical analyses and detailed investigations of individual stars. This offers the opportunity to study the full interior of the genuine hybrids, in which both low radial order p-and high-order g-modes are self-excited at the same time. However, a few other physical processes can also be responsible for the observed hybrid nature, related to binarity or to surface inhomogeneities. The finding that most delta Scuti stars also show long-period light variations represents a real challenge for theory.
Aims. We aim at determining the pulsation frequencies of KIC9533489, to search for regular patterns and spacings among them, and to investigate the stability of the frequencies and the amplitudes. An additional goal is to study the serendipitously detected transit events: is KIC9533489 the host star? What are the limitations on the physical parameters of the involved bodies?
Methods. We performed a Fourier analysis of all the available Kepler light curves. We investigated the frequency and period spacings and determined the stellar physical parameters from spectroscopic observations. We also modelled the transit events.
Results. The Fourier analysis of the Kepler light curves revealed 55 significant frequencies clustered into two groups, which are separated by a gap between 15 and 27 d(-1). The light variations are dominated by the beating of two dominant frequencies located at around 4 d(-1). The amplitudes of these two frequencies show a monotonic long-term trend. The frequency spacing analysis revealed two possibilities: the pulsator is either a highly inclined moderate rotator (v approximate to 70 km s(-1), i > 70 degrees) or a fast rotator (v approximate to 200 km s(-1)) with i approximate to 20 degrees. The transit analysis disclosed that the transit events that occur with a approximate to 197 d period may be caused by a 1.6 R-Jup body orbiting a fainter star, which would be spatially coincident with KIC9533489.
C1 [Bognar, Zs] MTA CSFK, Konkoly Observ, H-1121 Budapest, Hungary.
[Lampens, P.; Fremat, Y.; Sodor, A.; De Cat, P.] Koninklijke Sterrenwacht Belgie, B-1180 Brussels, Belgium.
[Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Isaacson, H. T.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Ciardi, D. R.] NASA, Exoplanet Sci Inst Caltech, Pasadena, CA 91125 USA.
[Gilliland, R. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Martin-Fernandez, P.] Univ Granada, Dept Fis Teor & Cosmos, E-18071 Granada, Spain.
RP Bognar, Z (reprint author), MTA CSFK, Konkoly Observ, Konkoly Thege Mu 15-17, H-1121 Budapest, Hungary.
EM bognar@konkoly.hu
FU Hungarian Eotvos Fellowship; ESA PECS [4000103541/11/NL/KML]; Belgian
Federal Science Policy [M0/33/029]; Hungarian Academy of Sciences;
MICINN of Spain [BES-2012-053246, AYA2011-24728]; Junta de Andalucia
[FQM-108]; NASA Science Mission directorate; W. M. Keck Foundation
FX The authors thank the anonymous referee for the constructive comments
and recommendations on the manuscript. Zs.B. acknowledges the support of
the Hungarian Eotvos Fellowship (2013), the kind hospitality of the
Royal Observatory of Belgium as a temporary voluntary researcher
(2013-2014), and, together with A.S., the support of the ESA PECS
project 4000103541/11/NL/KML. A.S. acknowledges support by the Belgian
Federal Science Policy (project M0/33/029, PI: P.D.C.) and by the Janos
Bolyai Research Scholarship of the Hungarian Academy of Sciences. P.M.F.
acknowledges support from MICINN of Spain via grants BES-2012-053246 and
AYA2011-24728, and from the "Junta de Andalucia" through the FQM-108
project. Funding for the Kepler mission is provided by the NASA Science
Mission directorate. We thank the Kepler team for the high-quality data
obtained by this outstanding mission. We are very grateful to Jorge
Jimenez Vicente (Universidad de Granada, Spain) and Evencio Mediavilla
(Instituto de Astrofisica de Canarias) for kindly providing a spectrum
with the INTEGRAL optical fiber system. Based on spectra obtained with
the HERMES spectrograph installed at the Mercator Telescope, operated by
the Flemish Community, with the Nordic Optical Telescope, operated by
the Nordic Optical Telescope Scientific Association, and with the
William Herschel Telescope, operated by the Isaac Newton Group of
Telescopes. All instruments are located at the Observatorio del Roque de
los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de
Canarias. 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
the National Aeronautics and Space Administration. The Observatory was
made possible by the generous financial support of the W. M. Keck
Foundation. The authors thank Simon Murphy for his useful comments on
the first version of this manuscript.
NR 62
TC 2
Z9 2
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2015
VL 581
AR A77
DI 10.1051/0004-6361/201526154
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1DX
UT WOS:000361803900077
ER
PT J
AU Fonti, S
Mancarella, F
Liuzzi, G
Roush, TL
Frouard, MC
Murphy, J
Blanco, A
AF Fonti, S.
Mancarella, F.
Liuzzi, G.
Roush, T. L.
Frouard, M. Chizek
Murphy, J.
Blanco, A.
TI Revisiting the identification of methane on Mars using TES data
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planets and satellites: atmospheres; astrobiology; methods: data
analysis; planets and satellites: terrestrial planets; techniques:
spectroscopic; infrared: planetary systems
ID MARTIAN ATMOSPHERE; SPECTROMETER DATA; UPPER LIMITS; IASI CODE;
SPECTROSCOPY; VARIABILITY; CHEMISTRY; SEARCH; RATIOS; LIFE
AB The presence and variability of methane in the Martian atmosphere has been investigated by several authors and spurred a lively discussion. In this context, we address our previous inference of spatial and temporal CH4 variability identified from Mars Global Surveyor Thermal Emission Spectrometer measurements which was used to suggest the possible existence of a martian methane cycle. The importance of the topic requires a clear assessment of such variability to correctly comprehend the possible production and destruction mechanisms of Martian methane. It is therefore important to carefully revisit previous results from a different perspective to confirm them before they are used for further investigations. We here describe in detail a new procedure used to validate these earlier Thermal Emission Spectrometer measurements and thoroughly analyze the results obtained with the revised procedure. In spite of our efforts of defining an efficient data analysis procedure, we have not been able to either confirm or refute the existence of the spatial and temporal variability of methane. Nevertheless, our work has produced new interesting tools, which, with the necessary adaptation, can be of some aid in processing and interpreting planetary spectra and, in general, for all the other cases requiring a preliminary selection of data included in very extensive datasets, which are difficult to be efficiently treated with traditional techniques.
C1 [Fonti, S.; Mancarella, F.; Blanco, A.] Univ Salento, Dipartimento Matemat & Fis E De Giorgi, I-73100 Lecce, Italy.
[Liuzzi, G.] Univ Basilicata, Scuola Ingn, I-85100 Potenza, Italy.
[Roush, T. L.] NASA, Ames Res Ctr, Planetary Syst Branch, Moffett Field, CA 94035 USA.
[Frouard, M. Chizek; Murphy, J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
RP Fonti, S (reprint author), Univ Salento, Dipartimento Matemat & Fis E De Giorgi, I-73100 Lecce, Italy.
EM sergio.fonti@le.infn.it
RI Liuzzi, Giuliano/M-1987-2015;
OI Liuzzi, Giuliano/0000-0003-3638-5750
FU Italian Space Agency (ASI); Italian Ministry of University and Research
FX S.F. and T.L.R. thank NASAs Visiting Research Associate program, at NASA
Headquarters, for enabling SF's visits to NASA Ames that were invaluable
for the completion of this effort. This research has been partially
supported by the Italian Space Agency (ASI) and the Italian Ministry of
University and Research.
NR 44
TC 1
Z9 1
U1 2
U2 11
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2015
VL 581
AR A136
DI 10.1051/0004-6361/201526235
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1DX
UT WOS:000361803900136
ER
PT J
AU Martinet, N
Bartlett, JG
Kiessling, A
Sartoris, B
AF Martinet, Nicolas
Bartlett, James G.
Kiessling, Alina
Sartoris, Barbara
TI Constraining cosmology with shear peak statistics: tomographic analysis
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gravitational lensing: weak; cosmological parameters
ID WEAK LENSING SURVEYS; PRIMORDIAL NON-GAUSSIANITY; DARK-MATTER HALOES;
COSMIC SHEAR; MASS FUNCTION; CLUSTERS; COVARIANCE
AB The abundance of peaks in weak gravitational lensing maps is a potentially powerful cosmological tool, complementary to measurements of the shear power spectrum. We study peaks detected directly in shear maps, rather than convergence maps, an approach that has the advantage of working directly with the observable quantity, the galaxy ellipticity catalog. Using large numbers of numerical simulations to accurately predict the abundance of peaks and their covariance, we quantify the cosmological constraints attainable by a large-area survey similar to that expected from the Euclid mission, focusing on the density parameter, Omega(m), and on the power spectrum normalization, sigma(8), for illustration. We present a tomographic peak counting method that improves the conditional (marginal) constraints by a factor of 1.2 (2) over those from a two-dimensional (i.e., non-tomographic) peak-count analysis. We find that peak statistics provide constraints an order of magnitude less accurate than those from the cluster sample in the ideal situation of a perfectly known observable-mass relation; however, when the scaling relation is not known a priori, the shear-peak constraints are twice as strong and orthogonal to the cluster constraints, highlighting the value of using both clusters and shear-peak statistics.
C1 [Martinet, Nicolas] Univ Paris 06, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Bartlett, James G.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, APC,CNRS IN2P3,CEA lrfu, F-75205 Paris 13, France.
[Martinet, Nicolas; Bartlett, James G.; Kiessling, Alina] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Sartoris, Barbara] Univ Trieste, Sez Astron, Dipartimento Fis, I-34143 Trieste, Italy.
[Sartoris, Barbara] INAF, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
RP Martinet, N (reprint author), Univ Paris 06, UMR 7095, Inst Astrophys Paris, 98bis Bd Arago, F-75014 Paris, France.
EM martinet@iap.fr
OI Kiessling, Alina/0000-0002-2590-1273
FU Ecole Normale Superieure de Cachan; Laboratoire AstroParticle et
Cosmologie; MIUR PRIN [J91J12000450001]; PRIN-MIUR [201278X4FL];
PRIN-INAF; inDark INFN Grant; Consorzio per la Fisica di Trieste
FX We are grateful to the anonymous referee for his/her careful reading and
helpful and constructive comments that improved the paper. N.M. thanks
the Ecole Normale Superieure de Cachan and the Laboratoire AstroParticle
et Cosmologie for financial support in the early stage of this work.
B.S. acknowledges financial support from MIUR PRIN2010-2011
(J91J12000450001), from the PRIN-MIUR 201278X4FL grant, from a
PRIN-INAF/2012 Grant, from the inDark INFN Grant and from the Consorzio
per la Fisica di Trieste. A portion 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.
NR 43
TC 4
Z9 4
U1 1
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2015
VL 581
AR A101
DI 10.1051/0004-6361/201425164
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1DX
UT WOS:000361803900101
ER
PT J
AU Venuti, L
Bouvier, J
Irwin, J
Stauffer, JR
Hillenbrand, LA
Rebull, LM
Cody, AM
Alencar, SHP
Micela, G
Flaccomio, E
Peres, G
AF Venuti, L.
Bouvier, J.
Irwin, J.
Stauffer, J. R.
Hillenbrand, L. A.
Rebull, L. M.
Cody, A. M.
Alencar, S. H. P.
Micela, G.
Flaccomio, E.
Peres, G.
TI UV variability and accretion dynamics in the young open cluster NGC 2264
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disks; stars: low-mass; stars: pre-main sequence;
stars: variables: T Tauri, Herbig Ae/Be; open clusters and associations:
individual: NGC 2264; ultraviolet: stars
ID T-TAURI STARS; TERM PHOTOMETRIC VARIABILITY; MAIN-SEQUENCE EVOLUTION;
SPITZER-SPACE-TELESCOPE; ORION NEBULA CLUSTER; MAGNETOSPHERIC ACCRETION;
LIGHT CURVES; DISK EVOLUTION; ROTOR-PROGRAM; AA TAURI
AB Context. Photometric variability is a distinctive feature of young stellar objects; exploring variability signatures at different wavelengths provides insight into the physical processes at work in these sources.
Aims. We explore the variability signatures at ultraviolet (UV) and optical wavelengths for several hundred accreting and nonaccreting members of the star-forming region NGC 2264 (similar to 3 Myr).
Methods. We performed simultaneous monitoring of u-and r-band variability for the cluster population with CFHT/MegaCam. The survey extended over two full weeks, with several flux measurements per observing night. A sample of about 750 young stars is probed in our study, homogeneously calibrated and reduced, with internally consistently derived stellar parameters. Objects span the mass range 0.1-2 M-circle dot; about 40% of them show evidence for active accretion based on various diagnostics (H-alpha, UV, and IR excesses).
Results. Statistically distinct variability properties are observed for accreting and non-accreting cluster members. The accretors exhibit a significantly higher level of variability than the non-accretors, in the optical and especially in the UV. The amount of u-band variability is found to correlate statistically with the median amount of UV excess in disk-bearing objects, which suggests that mass accretion and star-disk interaction are the main sources of variability in the u band. Spot models are applied to account for the amplitudes of variability of accreting and non-accreting members, which yields different results for each group. Cool magnetic spots, several hundred degrees colder than the stellar photosphere and covering from 5 to 30% of the stellar surface, appear to be the leading factor of variability for the non-accreting stars. In contrast, accretion spots with a temperature a few thousand degrees higher than the photospheric temperature and that extend over a few percent of the stellar surface best reproduce the variability of accreting objects. The color behavior is also found to be different between accreting and non-accreting stars. While objects commonly become redder when fainter, typical amplitudes of variability for accreting members rapidly increase from the r to the u band, which indicates a much stronger contrast at short wavelengths; a lower color dependence in the photometric amplitudes is instead measured for diskless stars. Finally, we compare the u-band variability monitored here on two-week timescales with that measured on both shorter (hours) and longer (years) timescales. We find that variability on timescales of hours is typically, 10% of the peak-to-peak variability on day timescales, while longer term variability on a timescale of years is consistent with amplitudes measured over weeks.
Conclusions. We conclude that for both accreting and non-accreting stars, the mid-term rotational modulation by hot and cold spots is the leading timescale for a variability of up to several years. In turn, this suggests that the accretion process is essentially stable over years, although it exhibits low-level shorter term variations in single accretion events.
C1 [Venuti, L.; Bouvier, J.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Venuti, L.; Bouvier, J.] CNRS, IPAG, F-38000 Grenoble, France.
[Venuti, L.; Peres, G.] Univ Palermo, Dipartimento Fis & Chim, I-90134 Palermo, Italy.
[Irwin, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stauffer, J. R.; Rebull, L. M.; Cody, A. M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Hillenbrand, L. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Cody, A. M.] NASA, Ames Res Ctr, Kepler Sci Off, Mountain View, CA 94035 USA.
[Alencar, S. H. P.] Univ Fed Minas Gerais, ICEx, Dept Fis, BR-30270901 Belo Horizonte, MG, Brazil.
[Micela, G.; Flaccomio, E.] Osservatorio Astron Palermo GS Vaiana, Ist Nazl Astrofis, I-90134 Palermo, Italy.
RP Venuti, L (reprint author), Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
EM Laura.Venuti@obs.ujf-grenoble.fr
OI Micela, Giuseppina/0000-0002-9900-4751; Flaccomio,
Ettore/0000-0002-3638-5788; PERES, Giovanni/0000-0002-6033-8180; Rebull,
Luisa/0000-0001-6381-515X
FU program LLP Erasmus at Universita degli Studi di Palermo; CNPq; CAPES;
Fapemig; [ANR 2011 Blanc SIMI5-6 020 01]
FX We thank the anonymous referee for useful comments. This publication
makes use of data products from the Sloan Digital Sky Survey. This
project was in part supported by the grant ANR 2011 Blanc SIMI5-6 020
01. L. V. acknowledges partial funding for this work from program LLP
Erasmus 2011/2012 at Universita degli Studi di Palermo. S.H.P.A.
acknowledges financial support from CNPq, CAPES and Fapemig.
NR 48
TC 10
Z9 10
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2015
VL 581
AR A66
DI 10.1051/0004-6361/201526164
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1DX
UT WOS:000361803900066
ER
PT J
AU Singh, G
Lozi, J
Guyon, O
Baudoz, P
Jovanovic, N
Martinache, F
Kudo, T
Serabyn, E
Kuhn, J
AF Singh, Garima
Lozi, Julien
Guyon, Olivier
Baudoz, Pierre
Jovanovic, Nemanja
Martinache, Frantz
Kudo, Tomoyuki
Serabyn, Eugene
Kuhn, Jonas
TI On-Sky Demonstration of Low-Order Wavefront Sensing and Control with
Focal Plane Phase Mask Coronagraphs
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID 1ST LIGHT; PRINCIPLE; SENSOR; SENSITIVITY
AB The ability to characterize exoplanets by spectroscopy of their atmospheres requires direct imaging techniques to isolate planet signal from the bright stellar glare. One of the limitations with the direct detection of exoplanets, either with ground- or space-based coronagraphs, is pointing errors and other low-order wavefront aberrations. The coronagraphic detection sensitivity at the diffraction limit therefore depends on how well low-order aberrations upstream of the focal plane mask are corrected. To prevent starlight leakage at the inner working angle of a phase mask coronagraph, we have introduced a Lyot-based low-order wavefront sensor (LLOWFS), which senses aberrations using the rejected starlight diffracted at the Lyot plane. In this article, we present the implementation, testing, and results of LLOWFS on the Subaru Coronagraphic Extreme Adaptive Optics system (SCExAO) at the Subaru Telescope. We have controlled 35 Zernike modes of a H-band vector vortex coronagraph in the laboratory and 10 Zernike modes on-sky with an integrator control law. We demonstrated a closed-loop pointing residual of 0.02 mas in the laboratory and 0.15 mas on-sky for data sampled using the minimal 2-s exposure time of the science camera. We have also integrated the LLOWFS in the visible high-order control loop of SCExAO, which in closed-loop operation has validated the correction of the noncommon path pointing errors between the infrared science channel and the visible wavefront sensing channel with pointing residual of 0.23 mas on-sky.
C1 [Singh, Garima; Lozi, Julien; Guyon, Olivier; Jovanovic, Nemanja; Kudo, Tomoyuki] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Singh, Garima; Baudoz, Pierre] Observ Paris, Lesia, F-92195 Meudon, France.
[Martinache, Frantz] Observ Cote Azur, F-06300 Nice, France.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kuhn, Jonas] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland.
RP Singh, G (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA.
RI Kuhn, Jonas/H-2338-2011
OI Kuhn, Jonas/0000-0002-6344-4835
FU MEXT, Japan
FX The SCExAO team would like to thank the AO188 scientists and engineers
for operating the AO system and diagnosing the issues faced during the
observations. We gratefully acknowledge the support and help from the
Subaru Observatory staff. This research is partly supported by a
Grant-in-Aid for Science Research in a Priority Area from MEXT, Japan.
NR 26
TC 5
Z9 5
U1 0
U2 4
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 SEP
PY 2015
VL 127
IS 955
BP 857
EP 869
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS9DB
UT WOS:000362388200005
ER
PT J
AU Jovanovic, N
Martinache, F
Guyon, O
Clergeon, C
Singh, G
Kudo, T
Garrel, V
Newman, K
Doughty, D
Lozi, J
Males, J
Minowa, Y
Hayano, Y
Takato, N
Morino, J
Kuhn, J
Serabyn, E
Norris, B
Tuthill, P
Schworer, G
Stewart, P
Close, L
Huby, E
Perrin, G
Lacour, S
Gauchet, L
Vievard, S
Murakami, N
Oshiyama, F
Baba, N
Matsuo, T
Nishikawa, J
Tamura, M
Lai, O
Marchis, F
Duchene, G
Kotani, T
Woillez, J
AF Jovanovic, N.
Martinache, F.
Guyon, O.
Clergeon, C.
Singh, G.
Kudo, T.
Garrel, V.
Newman, K.
Doughty, D.
Lozi, J.
Males, J.
Minowa, Y.
Hayano, Y.
Takato, N.
Morino, J.
Kuhn, J.
Serabyn, E.
Norris, B.
Tuthill, P.
Schworer, G.
Stewart, P.
Close, L.
Huby, E.
Perrin, G.
Lacour, S.
Gauchet, L.
Vievard, S.
Murakami, N.
Oshiyama, F.
Baba, N.
Matsuo, T.
Nishikawa, J.
Tamura, M.
Lai, O.
Marchis, F.
Duchene, G.
Kotani, T.
Woillez, J.
TI The Subaru Coronagraphic Extreme Adaptive Optics System: Enabling
High-Contrast Imaging on Solar-System Scales
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID PHASE-MASK CORONAGRAPH; GEMINI PLANET IMAGER; WAVE-FRONT SENSOR; HR
8799; 1ST LIGHT; SPECTROSCOPY; TELESCOPE; STAR; INTERFEROMETRY;
PERFORMANCE
AB The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument is a multipurpose high-contrast imaging platform designed for the discovery and detailed characterization of exoplanetary systems and serves as a testbed for high-contrast imaging technologies for ELTs. It is a multiband instrument which makes use of light from 600 to 2500 nm, allowing for coronagraphic direct exoplanet imaging of the inner 3 lambda/D from the stellar host. Wavefront sensing and control are key to the operation of SCExAO. A partial correction of low-order modes is provided by Subaru's facility adaptive optics system with the final correction, including high-order modes, implemented downstream by a combination of a visible pyramid wavefront sensor and a 2000-element deformable mirror. The well-corrected NIR (y-K bands) wavefronts can then be injected into anST of the available coronagraphs, including but not limited to the phase-induced amplitude apodization and the vector vortex coronagraphs, both of which offer an inner working angle as low as 1 lambda/D. Noncommon path, low-order aberrations are sensed with a coronagraphic low-order wavefront sensor in the infrared (IR). Low noise, high frame rate NIR detectors allow for active speckle nulling and coherent differential imaging, while the HAWAII 2RG detector in the HiCIAO imager and/or the CHARTS integral field spectrograph (from mid-2016) can take deeper exposures and/or perform angular, spectral, and polarimetric differential imaging. Science in the visible is provided by two interferometric modules: VAMPIRES and FIRST, which enable subdiffraction limited imaging in the visible region with polarimetric and spectroscopic capabilities respectively. We describe the instrument in detail and present preliminary results both on-sky and in the laboratory.
C1 [Jovanovic, N.; Guyon, O.; Clergeon, C.; Singh, G.; Kudo, T.; Doughty, D.; Lozi, J.; Minowa, Y.; Hayano, Y.; Takato, N.; Lai, O.] Subaru Telescope, Natl Astron Observ Japan, Hilo, HI 96720 USA.
[Jovanovic, N.; Norris, B.; Tuthill, P.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia.
[Martinache, F.] Observ Cote Azur, Blvd Observ, F-06304 Nice, France.
[Guyon, O.; Males, J.; Close, L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Guyon, O.; Newman, K.; Doughty, D.] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA.
[Singh, G.; Schworer, G.; Huby, E.; Perrin, G.; Lacour, S.; Gauchet, L.; Vievard, S.] Observ Paris, LESIA, F-92195 Meudon, France.
[Garrel, V.; Lai, O.] AURA, Gemini Observ, La Serena, Chile.
[Newman, K.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Morino, J.; Nishikawa, J.; Tamura, M.; Kotani, T.] Natl Astron Observ Japan, Mitaka, Tokyo, Japan.
[Kuhn, J.; Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Norris, B.; Tuthill, P.; Schworer, G.; Stewart, P.] Univ Sydney, Sch Phys, IPOS, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Huby, E.] Univ Liege, Dept Astrophys Geophys & Oceanographie, B-4000 Liege, Belgium.
[Murakami, N.; Oshiyama, F.; Baba, N.] Hokkaido Univ, Fac Engn, Div Appl Phys, Kita Ku, Sapporo, Hokkaido 0608628, Japan.
[Matsuo, T.] Kyoto Univ, Sakyo Ku, Kyoto 6068502, Japan.
[Tamura, M.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Lai, O.; Marchis, F.] Carl Sagan Ctr, SETT Inst, Mountain View, CA 94043 USA.
[Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Duchene, G.] Univ Grenoble Alpes, F-3800 Grenoble, France.
[Duchene, G.] CNRS, IPAG, F-3800 Grenoble, France.
[Woillez, J.] European So Observ, D-85748 Garching, Germany.
RP Jovanovic, N (reprint author), Subaru Telescope, Natl Astron Observ Japan, 650 N AOhoku Pl, Hilo, HI 96720 USA.
EM jovanovic.nem@gmail.com
RI Kuhn, Jonas/H-2338-2011
OI Kuhn, Jonas/0000-0002-6344-4835
FU Subaru directorate
FX We are grateful to B. Elms for his contributions to the fabrication of
parts for the SCExAO rebuild. The SCExAO team thanks the Subaru
directorate for funding various grants to realize and develop the
instrument.
NR 79
TC 38
Z9 38
U1 2
U2 8
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 SEP
PY 2015
VL 127
IS 955
BP 890
EP 910
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS9DB
UT WOS:000362388200008
ER
PT J
AU Bonet, B
Cavazza, M
desJardins, M
Felner, A
Hawes, N
Knox, B
Konidaris, G
Lang, J
Lopez, CL
Magazzeni, D
McGovern, A
Natarajan, S
Sturtevant, NR
Thielscher, M
Yeoh, W
Sardina, S
Wagstaff, K
AF Bonet, Blai
Cavazza, Marc
desJardins, Marie
Felner, Ariel
Hawes, Nick
Knox, Brad
Konidaris, George
Lang, Jerome
Linares Lopez, Carlos
Magazzeni, Daniele
McGovern, Amy
Natarajan, Sriraam
Sturtevant, Nathan R.
Thielscher, Michael
Yeoh, William
Sardina, Sebastian
Wagstaff, Kiri
TI A Summary of the Twenty-Ninth AAAI Conference on Artificial Intelligence
SO AI MAGAZINE
LA English
DT Article
AB The Twenty-Ninth AAAI Conference on Artificial Intelligence (AAAI-15) was held in January 2015 in Austin, Texas (USA) The conference program was cochaired by Sven Koenig and Blai Bonet. This report contains reflective summaries of the main conference, the robotics program, the AI and robotics workshop, the Virtual Agent Exhibition, the What's Hot track, the Competition Panel, the senior member track, student and outreach activities, the student abstract and poster program, the doctoral consortium, the women's mentoring event, and the demonstrations program.
C1 [Bonet, Blai] Univ Sidad Simon Bolivar, Comp Sci, Caracas, Venezuela.
[Cavazza, Marc] Univ Teesside, Sch Comp, Tees Valley, Middlesbrough, England.
[desJardins, Marie] Univ Maryland Baltimore Cty, Comp Sci, Baltimore, MD 21228 USA.
[Felner, Ariel] Ben Gurion Univ Negev, Beer Sheva, Israel.
[Hawes, Nick] Univ Birmingham, Sch Comp Sci, Autonomous Intelligent Robot, Birmingham B15 2TT, W Midlands, England.
[Knox, Brad] MIT, Cambridge, MA 02139 USA.
Univ So Calif, Comp Sci, Los Angeles, CA 90089 USA.
[Konidaris, George] Duke Univ, Comp sci, Durham, NC 27706 USA.
[Lang, Jerome] Univ Paris 09, CNRS, F-75775 Paris 16, France.
[Lang, Jerome] Univ Paris 09, Lamsade, F-75775 Paris 16, France.
[Linares Lopez, Carlos] Univ Carlos III Madrid, E-28903 Getafe, Spain.
[Magazzeni, Daniele] Kings Coll London, Comp Sci, London WC2R 2LS, England.
[McGovern, Amy] Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA.
[Natarajan, Sriraam] Indiana Univ, Sch Informat & Comp, Bloomington, IN 47405 USA.
[Sturtevant, Nathan R.] Univ Denver, Comp Sci Dept, Denver, CO 80208 USA.
[Thielscher, Michael] Univ New S Wales, Sch Comp Sci & Engn, Sydney, NSW 2052, Australia.
[Yeoh, William] Univ New Mexico, Dept Comp Sci, Albuquerque, NM 87131 USA.
[Sardina, Sebastian] RMIT Univ, Sch Comp Sci & Informat Technol, Melbourne, Vic, Australia.
[Wagstaff, Kiri] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Bonet, B (reprint author), Univ Sidad Simon Bolivar, Comp Sci, Caracas, Venezuela.
NR 0
TC 0
Z9 0
U1 1
U2 6
PU AMER ASSOC ARTIFICIAL INTELL
PI MENLO PK
PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA
SN 0738-4602
J9 AI MAG
JI AI Mag.
PD FAL
PY 2015
VL 36
IS 3
BP 99
EP 106
PG 8
WC Computer Science, Artificial Intelligence
SC Computer Science
GA CS2UD
UT WOS:000361926600009
ER
PT J
AU Ackermann, M
Ajello, M
Atwood, WB
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Gonzalez, JB
Bellazzini, R
Bissaldi, E
Blandford, RD
Bloom, ED
Bnino, R
Bottagini, E
Brandt, TJ
Bregeon, J
Britto, RJ
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caragiulo, M
Caraveo, PA
Careenter, B
Casandjian, JM
Cavazzuti, E
Cecchi, C
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Chiaro, G
Ciprini, S
Claus, R
Cohen-Tanugi, J
Cominsky, LR
Conrad, J
Cutini, S
D'Abrusco, R
D'Ammando, F
de Angelis, A
Desiante, R
Digel, SW
Di Venere, L
Drell, PS
FAvuzzi, C
Fegan, SJ
Ferrara, EC
Finke, J
Focke, WB
Franckowiak, A
Fuhrmann, L
Fukazawa, Y
Furniss, AK
Fusco, P
Gargano, E
Gasparrini, D
Giglietto, N
Giommi, P
Giordano, E
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grove, JE
Guiriec, S
Hewitt, JW
Hill, AB
Horan, D
Itoh, R
Johannesson, G
Johnson, AS
Johnson, WN
Kataoka, J
Kawano, T
Krauss, F
Kuss, M
La Mura, G
Larsson, S
Latronico, L
Leto, C
Li, J
Li, L
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Mayer, M
Mazziotta, MN
McEnery, JE
Michelson, PF
Mizuno, T
Moiseev, AA
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nuss, E
Ohno, M
Oxsugi, T
Ojha, R
Omdei, N
Orienti, M
Orlando, E
Paggi, A
Paneque, D
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Romani, RW
Salvetti, D
Schaal, M
Schinzel, FK
Schulz, A
Sgro, C
Siskind, EJ
Sokolovsky, KV
Spada, F
Spandre, G
Spinelli, P
Stawarz, L
Suson, DJ
Takahashi, H
Takahashi, T
Tanaka, Y
Thayer, JG
Thayer, JB
Tibaldo, L
Torres, DF
Torresi, E
Tosti, G
Troja, E
Uchiyama, Y
Vianello, G
Winer, BL
Wood, KS
Zimmer, S
AF Ackermann, M.
Ajello, M.
Atwood, W. B.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Gonzalez, J. Becerra
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bloom, E. D.
Bnino, R.
Bottagini, E.
Brandt, T. J.
Bregeon, J.
Britto, R. J.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caragiulo, M.
Caraveo, P. A.
Careenter, B.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Chiaro, G.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Cominsky, L. R.
Conrad, J.
Cutini, S.
D'Abrusco, R.
D'Ammando, F.
de Angelis, A.
Desiante, R.
Digel, S. W.
Di Venere, L.
Drell, P. S.
FAvuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Finke, J.
Focke, W. B.
Franckowiak, A.
Fuhrmann, L.
Fukazawa, Y.
Furniss, A. K.
Fusco, P.
Gargano, E.
Gasparrini, D.
Giglietto, N.
Giommi, P.
Giordano, E.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Hewitt, J. W.
Hill, A. B.
Horan, D.
Itoh, R.
Johannesson, G.
Johnson, A. S.
Johnson, W. N.
Kataoka, J.
Kawano, T.
Krauss, F.
Kuss, M.
La Mura, G.
Larsson, S.
Latronico, L.
Leto, C.
Li, J.
Li, L.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Mayer, M.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mizuno, T.
Moiseev, A. A.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nuss, E.
Ohno, M.
Oxsugi, T.
Ojha, R.
Omdei, N.
Orienti, M.
Orlando, E.
Paggi, A.
Paneque, D.
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.
Romani, R. W.
Salvetti, D.
Schaal, M.
Schinzel, F. K.
Schulz, A.
Sgro, C.
Siskind, E. J.
Sokolovsky, K. V.
Spada, F.
Spandre, G.
Spinelli, P.
Stawarz, L.
Suson, D. J.
Takahashi, H.
Takahashi, T.
Tanaka, Y.
Thayer, J. G.
Thayer, J. B.
Tibaldo, L.
Torres, D. F.
Torresi, E.
Tosti, G.
Troja, E.
Uchiyama, Y.
Vianello, G.
Winer, B. L.
Wood, K. S.
Zimmer, S.
TI THE THIRD CATALOG OF ACTIVE GALACTIC NUCLEI DETECTED BY THE FERMI LARGE
AREA TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: general; galaxies: active; galaxies: jets; gamma
rays: galaxies
ID GAMMA-RAY EMISSION; ALL-SKY SURVEY; EXTRAGALACTIC BACKGROUND LIGHT;
SPECTRUM RADIO QUASARS; GALAXY 3C 111; X-RAY; COMPLETE SAMPLE; OPTICAL
IDENTIFICATIONS; PARTICLE-ACCELERATION; RELATIVISTIC JETS
AB The third catalog of active galactic nuclei (AGNs) detected by the Fermi-LAT (3LAC) is presented. It is based on the third Fermi-LAT catalog (3FGL) of sources detected between 100 MeV and 300 GeV with a Test Statistic greater than 25, between 2008 August 4 and 2012 July 31. The 3LAC includes 1591 AGNs located at high Galactic latitudes (vertical bar b vertical bar > 10 degrees), a 71% increase over the second catalog based on 2 years of data. There are 28 duplicate associations, thus 1563 of the 2192 high-latitude gamma-ray sources of the 3FGL catalog are AGNs. Most of them (98%) are blazars. About half of the newly detected blazars are of unknown type, i.e., they lack spectroscopic information of sufficient quality to determine the strength of their emission lines. Based on their gamma-ray spectral properties, these sources are evenly split between flat-spectrum radio quasars (FSRQs) and BL Lacs. The most abundant detected BL Lacs are of the high-synchrotron-peaked (HSP) type. About 50% of the BL Lacs have no measured redshifts. A few new rare outliers (HSP-FSRQs and high-luminosity HSP BL Lacs) are reported. The general properties of the 3LAC sample confirm previous findings from earlier catalogs. The fraction of 3LAC blazars in the total population of blazars listed in BZCAT remains non-negligible even at the faint ends of the BZCAT-blazar radio, optical, and X-ray flux distributions, which hints that even the faintest known blazars could eventually shine in gamma-rays at LAT-detection levels. The energy-flux distributions of the different blazar populations are in good agreement with extrapolation from earlier catalogs.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.; Guiriec, S.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA.
[Atwood, W. B.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.] Ist Nazl Fis Nucl, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.] Univ Paris Diderot, Lab AIM, CEA IRFU, CNRS,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Desiante, R.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Chiaro, G.; La Mura, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Gonzalez, J. Becerra; Brandt, T. J.; Careenter, B.; Ferrara, E. C.; Guiriec, S.; McEnery, J. E.; Ojha, R.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gonzalez, J. Becerra; McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Gonzalez, J. Becerra; McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bellazzini, R.; Kuss, M.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bissaldi, E.; Caragiulo, M.; FAvuzzi, C.; Fusco, P.; Gargano, E.; Giglietto, N.; Giordano, E.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Blandford, R. D.; Bloom, E. D.; Bottagini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Furniss, A. K.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Johnson, A. S.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omdei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Vianello, G.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Blandford, R. D.; Bloom, E. D.; Bottagini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Furniss, A. K.; Glanzman, T.; Godfrey, G.; Hill, A. B.; Johnson, A. S.; Madejski, G. M.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omdei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Bnino, R.; Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bnino, R.] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy.
[Bregeon, J.; Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, F-34059 Montpellier, France.
[Britto, R. J.; Razzaque, S.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa.
[Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, Palaiseau, France.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caraveo, P. A.; Salvetti, D.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Careenter, B.] Catholic Univ Amer, Washington, DC 20064 USA.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] ASI Sci Data Ctr, I-00133 Rome, Italy.
[Cecchi, C.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Chekhtman, A.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA.
[Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA.
[Cheung, C. C.; Finke, J.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Ciprini, S.; Cutini, S.; Gasparrini, D.] INAF Osservatorio Astronom Roma, I-00040 Rome, Italy.
[Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA.
[Conrad, J.; Larsson, S.; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Conrad, J.; Larsson, S.; Li, L.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden.
[D'Abrusco, R.; Paggi, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Di Venere, L.; FAvuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, E.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Fuhrmann, L.; Sokolovsky, K. V.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Fukazawa, Y.; Itoh, R.; Kawano, T.; Ohno, M.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Hewitt, J. W.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Hewitt, J. W.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Hewitt, J. W.; Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA.
[Hewitt, J. W.; Moiseev, A. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Krauss, F.] Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany.
[La Mura, G.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[La Mura, G.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Leto, C.] ASI Sci Data Ctr, I-00044 Rome, Italy.
[Li, J.; Torres, D. F.] Inst Space Sci IEEC CSIC, E-08193 Barcelona, Spain.
[Li, L.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Lott, B.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, IN2P3 CNRS, F-33175 Gradignan, France.
[Mizuno, T.; Oxsugi, T.; Tanaka, Y.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Murgia, S.] Univ Calif Irvine, Phsics & Astron Dept, Ctr Cosmol, Irvine, CA 92697 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Schaal, M.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Schaal, M.] Naval Res Lab, Washington, DC 20375 USA.
[Schinzel, F. K.] Univ New Mexico, Albuquerque, NM 87131 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Sokolovsky, K. V.] Lebedev Phys Inst, Ctr Astro Space, Moscow 117810, Russia.
[Stawarz, L.; Takahashi, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Torresi, E.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.; Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
EM elisabetta.cavazzuti@asdc.asi.it; stefano.ciprini@asdc.asi.it;
sara.cutini@asdc.asi.it; gasparrini@asdc.asi.it; lott@cenbg.in2p3.fr
RI Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015;
Mazziotta, Mario /O-8867-2015; Morselli, Aldo/G-6769-2011; Reimer,
Olaf/A-3117-2013; giglietto, nicola/I-8951-2012; Moskalenko,
Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; D'Abrusco,
Raffaele/L-2767-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016;
Sokolovsky, Kirill/D-2246-2015; Paggi, Alessandro/C-1219-2017; Di
Venere, Leonardo/C-7619-2017
OI Gargano, Fabio/0000-0002-5055-6395; Bissaldi,
Elisabetta/0000-0001-9935-8106; Gasparrini, Dario/0000-0002-5064-9495;
Baldini, Luca/0000-0002-9785-7726; TORRESI,
ELEONORA/0000-0002-5201-010X; Becerra Gonzalez,
Josefa/0000-0002-6729-9022; Hill, Adam/0000-0003-3470-4834; Giordano,
Francesco/0000-0002-8651-2394; La Mura, Giovanni/0000-0001-8553-499X;
Caraveo, Patrizia/0000-0003-2478-8018; Sgro',
Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864;
Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti,
monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852;
Bonino, Raffaella/0000-0002-4264-1215; Johannesson,
Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673;
Mazziotta, Mario /0000-0001-9325-4672; Morselli,
Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; giglietto,
nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X;
D'Abrusco, Raffaele/0000-0003-3073-0605; Torres,
Diego/0000-0002-1522-9065; Sokolovsky, Kirill/0000-0001-5991-6863;
Paggi, Alessandro/0000-0002-5646-2410; Di Venere,
Leonardo/0000-0003-0703-824X
FU National Aeronautics and Space Administration; Department of Energy in
the United States; Commissariat a l'Energie Atomique; Centre National de
la Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France; Agenzia Spaziale Italiana; Istituto
Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture,
Sports, Science and Technology (MEXT); High Energy Accelerator Research
Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan;
K. A. Wallenberg Foundation; Swedish Research Council; Swedish National
Space Board in Sweden; National Science Foundation; Alfred P. Sloan
Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max
Planck Society; Higher Education Funding Council for England; American
Museum of Natural History; Astrophysical Institute Potsdam; University
of Basel; University of Cambridge; Case Western Reserve University;
University of Chicago; Drexel University; Fermilab; Institute for
Advanced Study; Japan Participation Group; Johns Hopkins University;
Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle
Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of
Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute
for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New
Mexico State University; Ohio State University; University of
Pittsburgh; University of Portsmouth; Princeton University; United
States Naval Observatory; University of Washington
FX The Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council, and the Swedish National Space Board in Sweden.
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France.r This
research has made use of data obtained from the high-energy Astrophysics
Science Archive Research Center (HEA-SARC) provided by NASA's Goddard
Space Flight Center; the SIMBAD database operated at CDS, Strasbourg,
France; and the NASA/IPAC Extragalactic Database (NED) operated by the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. This
research has made use of data archives, catalogs, and software tools
from the ASDC, a facility managed by the Italian Space Agency (ASI).
Part of this work is based on the NVSS. The National Radio Astronomy
Observatory is operated by Associated Universities, Inc., under contract
with the National Science Foundation. 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 publication makes use of data products from the
Wide-field Infrared Survey Explorer, which is a joint project of the
University of California, Los Angeles, and the Jet Propulsion
Laboratory/California Institute of Technology, funded by the National
Aeronautics and Space Administration. Funding for the SDSS and SDSS-II
has been provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Science Foundation, the U.S. Department of
Energy, the National Aeronautics and Space Administration, the Japanese
Monbukagakusho, the Max Planck Society, and the Higher Education Funding
Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS
is managed by the Astrophysical Research Consortium for the
Participating Institutions.; The Participating Institutions are the
American Museum of Natural History, Astrophysical Institute Potsdam,
University of Basel, University of Cambridge, Case Western Reserve
University, University of Chicago, Drexel University, Fermilab, the
Institute for Advanced Study, the Japan Participation Group, Johns
Hopkins University, the Joint Institute for Nuclear Astrophysics, the
Kavli Institute for Particle Astrophysics and Cosmology, the Korean
Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos
National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
Max-Planck-Institute for Astrophysics (MPA), New Mexico State
University, Ohio State University, University of Pittsburgh, University
of Portsmouth, Princeton University, the United States Naval
Observatory, and the University of Washington.
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JI Astrophys. J.
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900014
ER
PT J
AU Archibald, RF
Kaspi, VM
Beardmore, AP
Gehrels, N
Kennea, JA
AF Archibald, R. F.
Kaspi, V. M.
Beardmore, A. P.
Gehrels, N.
Kennea, J. A.
TI ON THE BRAKING INDEX OF THE UNUSUAL HIGH-B ROTATION-POWERED PULSAR PSR
J1846-0258
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (PSR J1846-0258); stars: neutron; X-rays: stars
ID X-RAY PULSAR; HIGH-MAGNETIC-FIELD; REMNANT KESTEVEN 75; SPIN-DOWN;
TIMING BEHAVIOR; NEUTRON-STARS; YOUNG PULSAR; 1E 1841-045; GLITCH;
EMISSION
AB PSR J1846-0258 is an object that straddles the boundary between magnetars and rotation powered pulsars. Though behaving for many years as a rotation-powered pulsar, in 2006, it exhibited distinctly magnetar-like behavior-emitting several short hard X-ray bursts, and a flux increase. Here we report on 7 years of post-outburst timing observations of PSR J1846-0258 using the Rossi X-ray Timing Explorer and the Swift X-ray Telescope. We measure the braking index over the post-magnetar outburst period to be n = 2.19 +/- 0.03. This represents a change of Delta n = -0.46 +/- 0.03 or a 14.5 sigma difference from the pre-outburst braking index of n = 2.65 +/- 0.01, which itself was measured over a span of 6.5 years. A change to a pulsar braking index so large and long-lived is unprecedented and poses a significant challenge to models of pulsar spin-down.
C1 [Archibald, R. F.; Kaspi, V. M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
RP Archibald, RF (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
OI Archibald, Robert/0000-0002-4017-8837
FU NSERC Alexander Graham Bell Canada Graduate Scholarship; Walter C.
Sumner Memorial Fellowship; NSERC; Centre de Recherche en Astrophysique
du Quebec; R. Howard Webster Foundation Fellowship from the Canadian
Institute for Advanced Study; Canada Research Chairs Program; Lorne
Trottier Chair in Astrophysics and Cosmology
FX R.F.A. acknowledges support from an NSERC Alexander Graham Bell Canada
Graduate Scholarship and a Walter C. Sumner Memorial Fellowship. V.M.K.
receives support from an NSERC Discovery Grant and Accelerator
Supplement, Centre de Recherche en Astrophysique du Quebec, an R. Howard
Webster Foundation Fellowship from the Canadian Institute for Advanced
Study, the Canada Research Chairs Program and the Lorne Trottier Chair
in Astrophysics and Cosmology. We thank R. Ferdman and E. Madsen for
useful discussions. We acknowledge the use of public data from the Swift
data archive. This research has made use of data obtained through the
High Energy Astrophysics Science Archive Research Center Online Service,
provided by the NASA/Goddard Space Flight Center.
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J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
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DI 10.1088/0004-637X/810/1/67
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900067
ER
PT J
AU Brosius, JW
Daw, AN
AF Brosius, Jeffrey W.
Daw, Adrian N.
TI QUASI-PERIODIC FLUCTUATIONS AND CHROMOSPHERIC EVAPORATION IN A SOLAR
FLARE RIBBON OBSERVED BY IRIS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: chromosphere; Sun: flares; Sun: UV radiation
ID ULTRAVIOLET IMAGING SPECTROMETER; BRAGG CRYSTAL SPECTROMETER; HIGH TIME
RESOLUTION; CORONAL DIAGNOSTIC SPECTROMETER; XIX RESONANCE LINE;
MAGNETIC RECONNECTION; EXTREME-ULTRAVIOLET; IMPULSIVE PHASE;
SPECTROSCOPIC OBSERVATIONS; ATOMIC DATABASE
AB The Interface Region Imaging Spectrograph (IRIS) satellite obtained rapid cadence (9.4 s) stare spectra of an M7 flare ribbon in AR 12036 on 2014 April 18. Chromospheric and transition region line emission exhibited quasi-periodic intensity and velocity fluctuations in the ribbon prior to the appearance of Fe XXI emission. Seven intensity peaks were observed in light curves from small (0 ''.333 x 0.'' 333) tracked spatial locations in the ribbon, the first four of which show variable time separations around 3 minutes, and the last four of which show variable time separations about half that value, i.e., the frequency appears to have doubled. The Fe XXI intensity increased rapidly and impulsively after the quasi-periodic fluctuations in chromospheric and transition region lines. The entire Fe XXI line profile was blueshifted when the line first appeared, corresponding to an upward velocity around -100 km s(-1). This upward velocity increased to a maximum of about -150 km s(-1) before diminishing to zero around the time of maximum intensity. Simultaneous, cospatial velocities observed with Si IV line emission were directed downward, consistent with explosive chromospheric evaporation. During this flare the Fe XXI line's profile is well fit with only one Gaussian component that is either wholly blueshifted or wholly at rest; no significant secondary blueshifted or redshifted components are observed. This suggests that IRIS may have sufficient spatial resolution to resolve loop strands in these flare observations. Under the assumption that the Fe XXI line is at rest when its width is thermal, we derive a rest wavelength of 1354.0714 +/- 0.0108 angstrom for this forbidden line.
C1 [Brosius, Jeffrey W.] Catholic Univ Amer, NASA Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Daw, Adrian N.] NASA Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
RP Brosius, JW (reprint author), Catholic Univ Amer, NASA Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA.
EM Jeffrey.W.Brosius@nasa.gov
FU Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract
FX IRIS is a NASA small explorer mission developed and operated by LMSAL
and partner institutions 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. CHIANTI is a collaborative project involving George Mason
University (USA), the University of Michigan (USA), and the University
of Cambridge (UK).
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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 SEP 1
PY 2015
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IS 1
DI 10.1088/0004-637X/810/1/45
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900045
ER
PT J
AU Dwek, E
Arendt, RG
AF Dwek, Eli
Arendt, Richard G.
TI THE EVOLUTION OF DUST MASS IN THE EJECTA OF SN 1987A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: general; Magellanic Clouds; supernovae:
individual (SN 1987A)
ID CORE-COLLAPSE SUPERNOVAE; BOLOMETRIC LIGHT-CURVE; II-P SUPERNOVAE; EARLY
UNIVERSE; HIGH-REDSHIFT; SOLAR NEIGHBORHOOD; CHEMICAL EVOLUTION;
SPACE-TELESCOPE; SN-1987A; REMNANT
AB We present a new analysis of the infrared (IR) emission from the ejecta of SN 1987A covering days 615, 775, 1144, 8515, and 9090 after the explosion. We show that the observations are consistent with the rapid formation of about 0.4 M-circle dot of dust, consisting of mostly silicates (MgS103), near day 615, and evolving to about 0.45 M. of composite dust grains consisting of similar to 0.4 M-circle dot of silicates and 0.05 M-circle dot of amorphous carbon after d circle dot ay similar to 8500. The proposed scenario challenges previous claims that dust in supernova (SN) ejecta is predominantly carbon, and that it grew from an initial mass of similar to 10(-3) M-circle dot, to over 0.5 M-circle dot by cold accretion. It alleviates several problems with previous interpretations of the data: (1) it reconciles the abundances of silicon, magnesium, and carbon with the upper limits imposed by nucleosynthesis calculations, (2) it eliminates the requirement that most of the dust observed around day 9000 grew by cold accretion onto the similar to 10(-3)M(circle dot) of dust previously inferred for days 615 and 775 after the explosion, and (3) establishes the dominance of silicate over carbon dust in the SN ejecta. At early epochs, the IR luminosit% of the dust is powered by the radioactive decay of Co-56, and at late times by at least (1.3-1.6) x 10(-4)M(circle dot) of Ti-44.
C1 [Dwek, Eli; Arendt, Richard G.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Arendt, Richard G.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
RP Dwek, E (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
EM eli.dwek@nasa.gov
OI Arendt, Richard/0000-0001-8403-8548
FU NASA [13-ADAP13-0094]
FX We thank Arkaprabha Sarangi for helpful discussions and the referee for
useful criticism that led to the improvement of the manuscript. This
work was supported by NASA Astrophysical Data Analysis Program
13-ADAP13-0094.
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EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2015
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IS 1
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PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900075
ER
PT J
AU Finkelstein, SL
Ryan, RE
Papovich, C
Dickinson, M
Song, MM
Somerville, RS
Ferguson, HC
Salmon, B
Giavalisco, M
Koekemoer, AM
Ashby, MLN
Behroozi, P
Castellano, M
Dunlop, JS
Faber, SM
Fazio, GG
Fontana, A
Grogin, NA
Hathi, N
Jaacks, J
Kocevski, DD
Livermore, R
McLure, RJ
Merlin, E
Mobasher, B
Newman, JA
Rafelski, M
Tilvi, V
Willner, SP
AF Finkelstein, Steven L.
Ryan, Russell E., Jr.
Papovich, Casey
Dickinson, Mark
Song, Mimi
Somerville, Rachel S.
Ferguson, Henry C.
Salmon, Brett
Giavalisco, Mauro
Koekemoer, Anton M.
Ashby, Matthew L. N.
Behroozi, Peter
Castellano, Marco
Dunlop, James S.
Faber, Sandy M.
Fazio, Giovanni G.
Fontana, Adriano
Grogin, Norman A.
Hathi, Nimish
Jaacks, Jason
Kocevski, Dale D.
Livermore, Rachael
McLure, Ross J.
Merlin, Emiliano
Mobasher, Bahram
Newman, Jeffrey A.
Rafelski, Marc
Tilvi, Vithal
Willner, S. P.
TI THE EVOLUTION OF THE GALAXY REST-FRAME ULTRAVIOLET LUMINOSITY FUNCTION
OVER THE FIRST TWO BILLION YEARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE early universe; galaxies: evolution; galaxies: formation; galaxies:
high-redshift; ultraviolet: galaxies
ID ULTRA-DEEP-FIELD; STAR-FORMING GALAXIES; SIMILAR-TO 7; HIGH-REDSHIFT
GALAXIES; LYMAN-BREAK GALAXIES; GOODS-SOUTH FIELD; EXTRAGALACTIC LEGACY
SURVEY; SPACE-TELESCOPE OBSERVATIONS; EMISSION-LINE GALAXIES; FORMATION
RATE DENSITY
AB We present a robust measurement and analysis of the rest-frame ultraviolet (UV) luminosity functions at z = 4-8. We use deep Hubble Space Telescope imaging over the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey/GOODS fields, the Hubble Ultra Deep Field, and the Hubble Frontier Field deep parallel observations near the Abell 2744 and MACS J0416.1-2403 clusters. The combination of these surveys provides an effective volume of 0.6-1.2 x 10(6) Mpc(3) over this epoch, allowing us to perform a robust search for faint (M-UV = -18) and bright (Muv < -21) high-redshift galaxies. We select candidate galaxies using a well-tested photometric redshift technique with careful screening of contaminants, finding a sample of 7446 candidate galaxies at 3.5 < z < 8.5, with >1000 galaxies at z approximate to 6-8. We measure both a stepwise luminosity function for candidate galaxies in our redshift samples, and a Schechter function, using a Markov Chain Monte Carlo analysis to measure robust uncertainties. At the faint end, our UV luminosity functions agree with previous studies, yet we find a higher abundance of UV-bright candidate galaxies at z >= 6. Our best-fit value of the characteristic magnitude MN is consistent with -21 at z >=, 5, which is different than that inferred based on previous trends at lower redshift, and brighter at similar to 2 sigma significance than previous measures at z = 6 and 7. At z = 8, a single power law provides an equally good fit to the UV luminosity function, while at z = 6 and 7 an exponential cutoff at the bright end is moderately preferred. We compare our luminosity functions to semi-analytical models, and find that the lack of evolution in M-UV(*) is consistent with models where the impact of dust attenuation on the bright end of the luminosity function decreases at higher redshift, although a decreasing impact of feedback may also be possible. We measure the evolution of the cosmic star-formation rate (SFR) density by integrating our observed luminosity functions to M-UV = -17, correcting for dust attenuation, and find that the SFR density declines proportionally to (1 +z)(-4.3 +/- 0 5) at z > 4, which is consistent with observations at z >= 9. Our observed luminosity functions are consistent with a reionization history that starts at z greater than or similar to 10, completes at z > 6, and reaches a midpoint (xH = 0.5) at 6.7 < z <9.4. Finally, using a constant cumulative number density selection and an empirically derived rising star-formation history, our observations predict that the abundance of bright z = 9 galaxies is likely higher than previous constraints, although consistent with recent estimates of bright z similar to 10 galaxies.
C1 [Finkelstein, Steven L.; Song, Mimi; Jaacks, Jason; Livermore, Rachael] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Ryan, Russell E., Jr.; Ferguson, Henry C.; Koekemoer, Anton M.; Behroozi, Peter; Grogin, Norman A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Papovich, Casey; Salmon, Brett; Tilvi, Vithal] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Dickinson, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Somerville, Rachel S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Giavalisco, Mauro] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Ashby, Matthew L. N.; Fazio, Giovanni G.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Castellano, Marco; Fontana, Adriano; Merlin, Emiliano] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Dunlop, James S.; McLure, Ross J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh, Midlothian, Scotland.
[Faber, Sandy M.] Univ Calif Santa Cruz, Lick Observ, Univ Calif Observ, Santa Cruz, CA 95064 USA.
[Hathi, Nimish] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Kocevski, Dale D.] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA.
[Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92512 USA.
[Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Newman, Jeffrey A.] Univ Pittsburgh, Pitt PACC, Pittsburgh, PA 15260 USA.
[Rafelski, Marc] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Finkelstein, SL (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
EM stevenf@astro.as.utexas.edu
RI Hathi, Nimish/J-7092-2014;
OI Hathi, Nimish/0000-0001-6145-5090; Castellano,
Marco/0000-0001-9875-8263; Papovich, Casey/0000-0001-7503-8482; Salmon,
Brett/0000-0002-7453-7279; Koekemoer, Anton/0000-0002-6610-2048
FU University of Texas at Austin College of Natural Sciences; NASA by
JPL/Caltech; ERC; NASA [NAS 5-26555]; NASA; [12060]
FX We thank Kristian Finlator, Brian Siana, Rychard Bouwens, Pascal Oesch,
Dan Jaffe, and Jon Trump for useful conversations. S.L.F. acknowledges
support from the University of Texas at Austin College of Natural
Sciences. M.S. was supported by a NASA Astrophysics and Data Analysis
Program award issued by JPL/Caltech. R.J.M. acknowledges ERC funding via
the award of a consolidator grant. This work is based on observations
made with the NASA/ESA Hubble Space Telescope, obtained at the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS
5-26555. These observations are associated with program #12060. This
work is also based in part on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. Support
for this work was provided by NASA through an award issued by
JPL/Caltech.
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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 SEP 1
PY 2015
VL 810
IS 1
DI 10.1088/0004-637X/810/1/71
PG 35
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900071
ER
PT J
AU Guo, JN
Zeitlin, C
Wimmer-Schweingruber, RF
Rafkin, S
Hassler, DM
Posner, A
Heber, B
Kohler, J
Ehresmann, B
Appel, JK
Bohm, E
Bottcher, S
Burmeister, S
Brinza, DE
Lohf, H
Martin, C
Kahanpaa, H
Reitz, G
AF Guo, Jingnan
Zeitlin, Cary
Wimmer-Schweingruber, Robert F.
Rafkin, Scot
Hassler, Donald M.
Posner, Arik
Heber, Bernd
Koehler, Jan
Ehresmann, Bent
Appel, Jan K.
Boehm, Eckart
Boettcher, Stephan
Burmeister, Soenke
Brinza, David E.
Lohf, Henning
Martin, Cesar
Kahanpaa, H.
Reitz, Guenther
TI MODELING THE VARIATIONS OF DOSE RATE MEASURED BY RAD DURING THE FIRST
MSL MARTIAN YEAR: 2012-2014
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: detectors; solar-terrestrial relations; space vehicles:
instruments
ID RADIATION ASSESSMENT DETECTOR; ENERGETIC PARTICLE RADIATION; CORONAL
ELECTRON-TEMPERATURE; PROTRACTED SOLAR MINIMUM; MAGNETIC-FIELD; SPACE
AGE; MARS; MODULATION; WIND; SURFACE
AB The Radiation Assessment Detector (RAD), on board Mars Science Laboratory's (MSL) rover Curiosity, measures the energy spectra of both energetic charged and neutral particles along with the radiation dose rate at the surface of Mars. With these first-ever measurements on the Martian surface, RAD observed several effects influencing the galactic cosmic-ray (GCR) induced surface radiation dose concurrently: (a) short-term diurnal variations of the Martian atmospheric pressure caused by daily thermal tides, (b) long-term seasonal pressure changes in the Martian atmosphere, and (c) the modulation of the primary GCR flux by the heliospheric magnetic field, which correlates with long-term solar activity and the rotation of the Sun. The RAD surface dose measurements, along with the surface pressure data and the solar modulation factor, are analyzed and fitted to empirical models that quantitatively demonstrate how the long-term influences ((b) and (c)) are related to the measured dose rates. Correspondingly, we can estimate dose rate and dose equivalents under different solar modulations and different atmospheric conditions, thus allowing empirical predictions of the Martian surface radiation environment.
C1 [Guo, Jingnan; Wimmer-Schweingruber, Robert F.; Heber, Bernd; Koehler, Jan; Appel, Jan K.; Boehm, Eckart; Boettcher, Stephan; Burmeister, Soenke; Lohf, Henning; Martin, Cesar] Univ Kiel, Inst Expt & Appl Phys, Kiel, Germany.
[Zeitlin, Cary] Southwest Res Inst, Earth Oceans & Space Dept, Durham, NH USA.
[Rafkin, Scot; Hassler, Donald M.; Ehresmann, Bent] Southwest Res Inst, Space Sci & Engn Div, Boulder, CO USA.
[Posner, Arik] NASA Headquarters, Sci Miss Directorate, Washington, DC USA.
[Brinza, David E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Kahanpaa, H.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Reitz, Guenther] Deutsch Zentrum Luft & Raumfahrt, Aerosp Med, Cologne, Germany.
RP Guo, JN (reprint author), Univ Kiel, Inst Expt & Appl Phys, Kiel, Germany.
EM guo@physik.uni-kiel.de
OI Kahanpaa, Henrik/0000-0001-9108-186X; Wimmer-Schweingruber,
Robert/0000-0002-7388-173X
FU National Aeronautics and Space Administration (NASA, HEOMD) under Jet
Propulsion Laboratory (JPL) [1273039]; DLR and DLR's Space
Administration [50QM0501, 50QM1201]; NASA
FX RAD is supported by the National Aeronautics and Space Administration
(NASA, HEOMD) under Jet Propulsion Laboratory (JPL) subcontract #1273039
to Southwest Research Institute and in Germany by DLR and DLR's Space
Administration grant numbers 50QM0501 and 50QM1201 to the Christian
Albrechts University, Kiel. Part of this research was carried out at
JPL, California Institute of Technology, under a contract with NASA. The
sunspot data have been obtained from WDC-SILSO, Royal Observatory of
Belgium, Brussels. We are grateful to the Cosmic Ray Station of the
University of Oulu and Sodankyla Geophysical Observatory for sharing
their Neutron Monitor count rate data. The data used in this paper are
archived in the NASA Planetary Data Systems Planetary Plasma
Interactions Node at the University of California, Los Angeles. The
archival volume includes the full binary raw data files, detailed
descriptions of the structures therein, and higher-level data products
in human-readable form. The PPI node is hosted at
http://ppi.pds.nasa.gov/.
NR 53
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2015
VL 810
IS 1
AR 24
DI 10.1088/0004-637X/810/1/24
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900024
ER
PT J
AU Hamren, KM
Rockosi, CM
Guhathakurta, P
Boyer, ML
Smith, GH
Dalcanton, JJ
Gregersen, D
Seth, AC
Lewis, AR
Williams, BF
Toloba, E
Girardi, L
Dorman, CE
Gilbert, KM
Weisz, DR
AF Hamren, Katherine M.
Rockosi, Constance M.
Guhathakurta, Puragra
Boyer, Martha L.
Smith, Graeme H.
Dalcanton, Julianne J.
Gregersen, Dylan
Seth, Anil C.
Lewis, Alexia R.
Williams, Benjamin F.
Toloba, Elisa
Girardi, Leo
Dorman, Claire E.
Gilbert, Karoline M.
Weisz, Daniel R.
TI A SPECTROSCOPIC AND PHOTOMETRIC EXPLORATION OF THE C/M RATIO IN THE DISK
OF M31
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: stellar content; Local Group; stars: AGB and post-AGB
ID ASYMPTOTIC GIANT BRANCH; LOCAL GROUP GALAXIES; CARBON STAR SURVEY; H-II
REGIONS; AGB STARS; MAGELLANIC CLOUDS; STELLAR CONTENT; EVOLVED STARS;
HII-REGIONS; METALLICITY
AB We explore the ratio (C/M) of carbon-rich to oxygen-rich thermally pulsing asymptotic giant branch (TP-AGB) stars in the disk of M31 using a combination of moderate-resolution optical spectroscopy from the Spectroscopic Landscape of Andromeda's Stellar Halo survey and six-filter Hubble Space Telescope photometry from the Panchromatic Hubble Andromeda Treasury survey. Carbon stars were identified spectroscopically. Oxygen-rich M-stars were identified using three different photometric definitions designed to mimic, and thus evaluate, selection techniques common in the literature. We calculate the C/M ratio as a function of galactocentric radius, present-day gas-phase oxygen abundance, stellar metallicity, age (via proxy defined as the ratio of TP-AGB stars to red giant branch, stars), and mean star formation rate over the last 400 Myr. We find statistically significant correlations between log(C/M) and all parameters. These trends are consistent across different M-star selection methods, though the fiducial values change. Of particular note is our observed relationship between log(C/M) and stellar metallicity, which is fully consistent with the trend seen across Local Group satellite galaxies. The fact that this trend persists in stellar populations with very different star formation histories indicates that the C/M ratio is governed by stellar properties alone.
C1 [Hamren, Katherine M.; Rockosi, Constance M.; Guhathakurta, Puragra; Smith, Graeme H.; Toloba, Elisa; Dorman, Claire E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Boyer, Martha L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Dalcanton, Julianne J.; Lewis, Alexia R.; Williams, Benjamin F.; Weisz, Daniel R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Gregersen, Dylan; Seth, Anil C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Girardi, Leo] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Gilbert, Karoline M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Hamren, KM (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA.
EM khamren@ucolick.org
OI Seth, Anil/0000-0003-0248-5470; Weisz, Daniel/0000-0002-6442-6030
FU NSF [AST-1010039, AST-1412648]; NASA [HST-GO-12055]; NASA through Hubble
Fellowship [HST-HF-51331.01]; Space Telescope Science Institute
FX P.G. and K.H. acknowledge NSF grants AST-1010039 and AST-1412648. This
work was also supported by NASA grant HST-GO-12055. K.H. was supported
by a NSF Graduate Research Fellowship. D.R.W. is supported by NASA
through Hubble Fellowship grant HST-HF-51331.01 awarded by the Space
Telescope Science Institute. We thank Bernhard Aringer, Zachary
Jennings, and Alex Rudy for helpful conversations. We appreciate the
very significant cultural role and reverence that the summit of Mauna
Kea has always had within the indigenous Hawaiian community. We are most
grateful to have had the opportunity to conduct observations from this
mountain.
NR 62
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2015
VL 810
IS 1
DI 10.1088/0004-637X/810/1/60
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900060
ER
PT J
AU Hippke, M
Angerhausen, D
AF Hippke, Michael
Angerhausen, Daniel
TI PHOTOMETRY'S BRIGHT FUTURE: DETECTING SOLAR SYSTEM ANALOGS WITH FUTURE
SPACE TELESCOPES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: detection
ID EXTRASOLAR GIANT PLANETS; SUN-LIKE STAR; LIGHT CURVES; FUNDAMENTAL
PROPERTIES; II. APPLICATION; KEPLER PLANETS; M-DWARF; TRANSIT; STELLAR;
NOISE
AB Time-series transit photometry from the Kepler space telescope has allowed for the discovery of thousands of exoplanets. We explore the potential of yet improved future missions such as PLATO 2.0 in detecting solar system analogs. We use real-world solar data and end-to-end simulations to explore the stellar and instrumental noise properties. By injecting and retrieving planets, rings, and moons of our own solar system, we show that the discovery of Venus. and Earth. analogs transiting G. dwarfs like our Sun is feasible at high signal-to-noise ratio after collecting 6 yr. of data, but Mars and Mercury analogs will be difficult to detect owing to stellar noise. In the best cases, Saturn's rings and Jupiter's moons will be detectable even in single-transit observations. Through the high number (> 1 billion) of observed stars by PLATO 2.0, it will become possible to detect thousands of single-transit events by cold gas giants, analogs. to our Jupiter, Saturn, Uranus, and Neptune. Our own solar system aside, we also show, through signal injection and retrieval, that PLATO 2.0. class photometry will allow for the secure detection of exomoons transiting quiet M. dwarfs. This is the first study analyzing in. depth the potential of future missions. and the ultimate limits of photometry, using realistic case examples.
C1 [Hippke, Michael] Inst Data Anal, D-47506 Neukirchen Vluyn, Germany.
[Angerhausen, Daniel] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hippke, M (reprint author), Inst Data Anal, Luiter Str 21b, D-47506 Neukirchen Vluyn, Germany.
EM hippke@ifda.eu; daniel.angerhausen@nasa.gov
FU NASA
FX We thank Jason W. Barnes and Jorge Zuluaga for their help with
understanding diffractive forward. scattering during the transit of
Saturn's rings, and Wei Zhu for providing data for modeling oblateness.
D.A.'s research was supported by an appointment to the NASA Postdoctoral
Program at the NASA Goddard Space Flight Center administered by Oak
Ridge Associated Universities through a contract with NASA.
NR 100
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2015
VL 810
IS 1
AR 29
DI 10.1088/0004-637X/810/1/29
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900029
ER
PT J
AU Huppenkothen, D
Brewer, BJ
Hogg, DW
Murray, I
Frean, M
Elenbaas, C
Watts, AL
Levin, Y
Van Der Horst, AJ
Kouveliotou, C
AF Huppenkothen, Daniela
Brewer, Brendon J.
Hogg, David W.
Murray, Iain
Frean, Marcus
Elenbaas, Chris
Watts, Anna L.
Levin, Yuri
Van Der Horst, Alexander J.
Kouveliotou, Chryssa
TI DISSECTING MAGNETAR VARIABILITY WITH BAYESIAN HIERARCHICAL MODELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; methods: statistical; pulsars: individual (SGR
J1550-5418); stars: magnetars; stars: magnetic field; X-rays: bursts
ID RAY BURST MONITOR; SELF-ORGANIZED CRITICALITY; PULSAR 1E 1547.0-5408;
SOFT GAMMA-REPEATERS; X-RAY; NEUTRON-STARS; SGR J1550-5418;
SPATIOTEMPORAL EVOLUTION; STATISTICAL PROPERTIES; RADIATIVE MECHANISM
AB Neutron stars are a prime laboratory for testing physical processes under conditions of strong gravity, high density, and extreme magnetic fields. Among the zoo of neutron star phenomena, magnetars stand out for their bursting behavior, ranging from extremely bright, rare giant flares to numerous, less energetic recurrent bursts. The exact trigger and emission mechanisms for these bursts are not known; favored models involve either a crust fracture and subsequent energy release into the magnetosphere, or explosive reconnection of magnetic field lines. In the absence of a predictive model, understanding the physical processes responsible for magnetar burst variability is difficult. Here, we develop an empirical model that decomposes magnetar bursts into a superposition of small spike-like features with a simple functional form, where the number of model components is itself part of the inference problem. The cascades of spikes that we model might be formed by avalanches of reconnection, or crust rupture aftershocks. Using Markov Chain Monte Carlo sampling augmented with reversible jumps between models with different numbers of parameters, we characterize the posterior distributions of the model parameters and the number of components per burst. We relate these model parameters to physical quantities in the system, and show for the first time that the variability within a burst does not conform to predictions from ideas of self-organized criticality. We also examine how well the properties of the spikes fit the predictions of simplified cascade models for the different trigger mechanisms.
C1 [Huppenkothen, Daniela; Elenbaas, Chris; Watts, Anna L.; Van Der Horst, Alexander J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Huppenkothen, Daniela; Hogg, David W.] NYU, Ctr Data Sci, New York, NY 10003 USA.
[Huppenkothen, Daniela; Hogg, David W.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Brewer, Brendon J.] Univ Auckland, Dept Stat, Auckland 1142, New Zealand.
[Murray, Iain] Univ Edinburgh, Sch Informat, Edinburgh EH8 9AB, Midlothian, Scotland.
[Frean, Marcus] Victoria Univ Wellington, Sch Engn & Comp Sci, Wellington, New Zealand.
[Levin, Yuri] Monash Univ, Monash Ctr Astrophys, Clayton, Vic 3800, Australia.
[Levin, Yuri] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Astrophys Off, Huntsville, AL 35812 USA.
[Kouveliotou, Chryssa] NSSTC, Huntsville, AL 35805 USA.
RP Huppenkothen, D (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands.
EM daniela.huppenkothen@nyu.edu
FU Netherlands Organization for Scientific Research (NWO); Moore-Sloan Data
Science Environment at NYU; Marsden Fast Start grant from the Royal
Society of New Zealand; NOVA Network 4; Monash Reaseach Acceleration
grant; European Research Council [247295]; NASA [NNH07ZDA001-GLAST]
FX D.H., B.J.B., D.W.H., M.F., and I.M. thank the organizers of MaxEnt2013,
and also thank Ewan Cameron for valuable input to this project. D.H. was
partially supported by a Netherlands Organization for Scientific
Research (NWO) Vidi Fellowship (PI A. Watts) and the Moore-Sloan Data
Science Environment at NYU. B.J.B. is supported by a Marsden Fast Start
grant from the Royal Society of New Zealand. C.E. acknowledges funding
from NOVA Network 4. Y.L. acknowledges support from a Monash Reaseach
Acceleration grant. A.J.v.d.H. acknowledges support from the European
Research Council via Advanced Investigator grant No. 247295 (PI:
R.A.M.J. Wijers). C.K. and was partially supported by NASA grant
NNH07ZDA001-GLAST.
NR 74
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2015
VL 810
IS 1
DI 10.1088/0004-637X/810/1/66
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900066
ER
PT J
AU Riemer-Sorensen, S
Wik, D
Madejski, G
Molendi, S
Gastaldello, F
Harrison, FA
Craig, WW
Hailey, CJ
Boggs, SE
Christensen, FE
Stern, D
Zhang, WW
Hornstrup, A
AF Riemer-Sorensen, S.
Wik, D.
Madejski, G.
Molendi, S.
Gastaldello, F.
Harrison, F. A.
Craig, W. W.
Hailey, C. J.
Boggs, S. E.
Christensen, F. E.
Stern, D.
Zhang, W. W.
Hornstrup, A.
TI DARK MATTER LINE EMISSION CONSTRAINTS FROM NuSTAR OBSERVATIONS OF THE
BULLET CLUSTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; line: identification; X-rays: galaxies: clusters
ID MASSIVE GALAXY CLUSTERS; XMM-NEWTON OBSERVATIONS; X-RAY-SPECTRA; STERILE
NEUTRINOS; URSA-MINOR; MILKY-WAY; LOW-COUNT; WILLMAN 1; SEARCH;
COSMOLOGY
AB Some dark matter candidates, e.g., sterile neutrinos, provide observable signatures in the form of mono-energetic line emission. We present the first search for dark matter line emission in the 3-80 keV range in a pointed observation of the Bullet Cluster with NuSTAR. We do not detect any significant line emission and instead we derive upper limits (95% CL) on the flux, and interpret these constraints in the context of sterile neutrinos and more generic dark matter candidates. NuSTAR does not have the sensitivity to constrain the recently claimed line detection at 3.5 keV, but improves on the constraints for energies of 10-25 keV.
C1 [Riemer-Sorensen, S.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway.
[Wik, D.; Zhang, W. W.] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Madejski, G.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[Molendi, S.; Gastaldello, F.] IASF Milano, INAF, I-20133 Milan, Italy.
[Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Craig, W. W.; Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Christensen, F. E.; Hornstrup, A.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Riemer-Sorensen, S (reprint author), Univ Oslo, Inst Theoret Astrophys, PO 1029, NO-0315 Oslo, Norway.
EM signe.riemer-sorensen@astro.uio.no
RI Gastaldello, Fabio/N-4226-2015; Boggs, Steven/E-4170-2015;
OI Gastaldello, Fabio/0000-0002-9112-0184; Boggs,
Steven/0000-0001-9567-4224; Riemer-Sorensen, Signe/0000-0002-5308-7651;
Molendi, Silvano/0000-0002-2483-278X
FU NASA
FX This research made use of data from the NuSTAR mission, a project led by
the California Institute of Technology, managed by the Jet Propulsion
Laboratory, and funded by NASA, and it also 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 54
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2015
VL 810
IS 1
DI 10.1088/0004-637X/810/1/48
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900048
ER
PT J
AU Sahai, R
Sanz-Forcada, J
Contreras, CS
Stute, M
AF Sahai, R.
Sanz-Forcada, J.
Sanchez Contreras, C.
Stute, M.
TI A PILOT DEEP SURVEY FOR X-RAY EMISSION FROM fuvAGB STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; binaries: symbiotic; circumstellar matter; stars: AGB
and post-AGB; stars: individual (EY, Hya, Y, Gem, CI, Hyi); stars:
mass-loss
ID GIANT BRANCH STARS; PLANETARY-NEBULAE; MAGNETIC-FIELDS; AGB STARS;
ACCRETION; TEMPERATURES; SYSTEM; GALEX; JETS; M6
AB We report the results of a pilot survey for X-ray emission from a newly discovered class of AGB stars with farultraviolet excesses (fuvAGB stars) using XMM-Newton and Chandra. We detected X-ray emission in three of six fuvAGB stars observed the X-ray fluxes are found to vary in a stochastic or quasi-periodic manner on roughly hour-long timescales, and simultaneous UV observations using the Optical Monitor on XMM for these sources show similar variations in the UV flux. These data, together with previous studies, show that X-ray emission is found only in fuvAGB stars. From modeling the spectra, we find that the observed X-ray luminosities are similar to(0.002-0.2) L-circle dot and the X-ray-emitting plasma temperatures are 05-160) x 106K. The high X-ray temperatures argue against the emission arising in stellar coronae, or directly in an accretion shock, unless it occurs on a WD companion. However, none of the detected objects is a known WD-symbiotic star, suggesting that if WD companions are present, they are relatively cool (<20,000 K). In addition, the high X-ray luminosities specifically argue against emission originating in the coronae of main-sequence companions. We discuss several models for the X-ray emission and its variability and find that the most likely scenario for the origin of the X-ray (and FUV) emission involves accretion activity around a companion star, with confinement by strong magnetic fields associated with the companion and/or an accretion disk around it.
C1 [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sanz-Forcada, J.; Sanchez Contreras, C.] CSIC INTA, Astrobiol Ctr, E-28691 Madrid, Spain.
[Stute, M.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA.
RI Sanchez-Contreras, Carmen/N-3718-2015; Sanz-Forcada, Jorge/C-3176-2017
OI Sanchez-Contreras, Carmen/0000-0002-6341-592X; Sanz-Forcada,
Jorge/0000-0002-1600-7835
FU NASA; NASA [GO4-15010Z, NAS5-26555]; Spanish MINECO [CSD2009-00038,
AYA2009-07304, AYA2012-32032]; NASA Office of Space Science
[NNX09AF08G]; [AYA2011-30147-C03-03]
FX We would like to thank an anonymous referee whose review has led to
substantial improvements in an earlier version of this paper. We also
thank Neal Turner for helpful discussions. R.S.'s contribution to the
research described here was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA. Financial support was provided by NASA, in part from award
GO4-15010Z for Chandra Cycle 15 proposal 15200476 and an ADAP award to
R.S. C.S.C.'s work is partially supported by Spanish MINECO through
grants CSD2009-00038, AYA2009-07304, and AYA2012-32032. J.S.F.
acknowledges funding from grant AYA2011-30147-C03-03. Some of the data
presented in this paper were obtained from the Mikulski Archive for
Space Telescopes (MAST) at STScI. 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 30
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2015
VL 810
IS 1
DI 10.1088/0004-637X/810/1/77
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900077
ER
PT J
AU Schwieterman, EW
Robinson, TD
Meadows, VS
Misra, A
Domagal-Goldman, S
AF Schwieterman, Edward W.
Robinson, Tyler D.
Meadows, Victoria S.
Misra, Amit
Domagal-Goldman, Shawn
TI DETECTING AND CONSTRAINING N-2 ABUNDANCES IN PLANETARY ATMOSPHERES USING
COLLISIONAL PAIRS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; Earth; planets and satellites: atmospheres; planets and
satellites: terrestrial planets; techniques: spectroscopic
ID 4.3 MU-M; TRANSMISSION SPECTROSCOPY; TERRESTRIAL PLANETS; EARTHS
ATMOSPHERE; SUPER-EARTHS; M-DWARFS; INDUCED ABSORPTION; HABITABLE ZONES;
SPECTRA; RETRIEVAL
AB Characterizing the bulk atmosphere of a terrestrial planet is important for determining surface pressure and potential habitability. Molecular nitrogen (N-2) constitutes the largest fraction of Earth's atmosphere and is likely to be a major constituent of many terrestrial exoplanet atmospheres. Due to its lack of significant absorption features, N-2 is extremely difficult to remotely detect. However, N-2 produces an N-2 N-2 collisional Pair, (N-2)(2), which is spectrally active. Here we report the detection of (N-2)(2) in Earth's disk-integrated spectrum. By comparing spectra from NASA's EPDXI mission to synthetic spectra from the NASA Astrobiology Institute's Virtual Planetary Laboratory threedimensional spectral Earth model, we find that (N-2)(2) absorption produces a 35% decrease in flux at 4.15 pm. Quantifying N-2 could provide a means of determining bulk atmospheric composition for terrestrial exoplanets and could rule out abiotic O-2 generation, which is possible in rarefied atmospheres. To explore the potential effects of (N-2)(2) in exoplanet spectra, we used radiative transfer models to generate synthetic emission and transit transmission spectra of self-consistent N-2-CO2 H2O atmospheres, and analytic N-2-H-2 and N-2-H-2-CO2 atmospheres. We show that (N-2)(2) absorption in the wings of the 4.3 pm CO2 band is strongly dependent on N-2 partial pressures above 0.5 bar and can significantly widen this band in thick N-2 atmospheres. The (N-2)(2) transit transmission signal is up to 10 ppm for an Earth-size planet with an N-2-dominated atmosphere orbiting within the habitable zone of an M5V star and could be substantially larger for planets with significant H-2 mixing ratios.
C1 [Schwieterman, Edward W.; Meadows, Victoria S.; Misra, Amit] Univ Washington, Dept Astron, Seattle, WA 98115 USA.
[Schwieterman, Edward W.; Robinson, Tyler D.; Meadows, Victoria S.; Misra, Amit; Domagal-Goldman, Shawn] NAI Virtual Planetary Lab, Seattle, WA 98115 USA.
[Schwieterman, Edward W.; Meadows, Victoria S.; Misra, Amit] Univ Washington, Astrobiol Program, Seattle, WA 98115 USA.
[Robinson, Tyler D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Domagal-Goldman, Shawn] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Schwieterman, EW (reprint author), Univ Washington, Dept Astron, Seattle, WA 98115 USA.
EM eschwiet@uw.edu
OI Schwieterman, Edward/0000-0002-2949-2163; Domagal-Goldman,
Shawn/0000-0003-0354-9325
FU NASA Astrobiology Institute's Virtual Planetary Laboratory - NASA
Astrobiology Institute [NNH12ZDA002C, NNA13AA93A]; NASA Ames Research
Center
FX This work was supported by the NASA Astrobiology Institute's Virtual
Planetary Laboratory Lead Team, funded through the NASA Astrobiology
Institute under solicitation NNH12ZDA002C and Cooperative Agreement
Number NNA13AA93A. T.R. gratefully acknowledges support from an
appointment to the NASA Postdoctoral Program at NASA Ames Research
Center, administered by Oak Ridge Affiliated Universities. This work
benefited from the use of advanced computational, storage, and
networking infrastructure provided by the Hyak supercomputer system at
the University of Washington. This research has made use of NASA's
Astrophysics Data System. We thank Dave Crisp and Robin Wordsworth for
helpful comments and discussion. We are grateful for the comments of an
anonymous reviewer, which allowed us to greatly improve this manuscript.
NR 73
TC 9
Z9 9
U1 2
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2015
VL 810
IS 1
DI 10.1088/0004-637X/810/1/57
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900057
ER
PT J
AU Simitev, RD
Kosovichev, AG
Busse, FH
AF Simitev, Radostin D.
Kosovichev, Alexander G.
Busse, Friedrich H.
TI DYNAMO EFFECTS NEAR THE TRANSITION FROM SOLAR TO ANTI-SOLAR DIFFERENTIAL
ROTATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE convection; dynamo; magnetohydrodynamics (MHD); stars: magnetic field;
Sun: magnetic fields; Sun: rotation
ID SPHERICAL FLUID SHELLS; STELLAR CONVECTION ZONES; TURBULENT CONVECTION;
ANELASTIC CONVECTION; THERMAL-CONVECTION; DRIVEN DYNAMOS; ZONAL FLOW;
COOL STARS; SIMULATIONS; GEODYNAMO
AB Numerical MHD simulations play an increasingly important role for understanding the mechanisms of stellar magnetism. We present simulations of convection and dynamos in density-stratified rotating spherical fluid shells. We employ a new 3D simulation code for obtaining the solution of a physically consistent anelastic model of the process with a minimum number of parameters. The reported dynamo simulations extend into a "buoyancy-dominated" regime where the buoyancy forcing is dominant while the Coriolis force is no longer balanced by pressure gradients, and strong anti-solar differential rotation develops as a result. We find that the self-generated magnetic fields, despite being relatively weak, are able to reverse the direction of differential rotation from anti-solar to solar-like. We also find that convection flows in this regime are significantly stronger in the polar regions than in the equatorial region, leading to non-oscillatory dipole-dominated dynamo solutions, and to a concentration of magnetic field in the polar regions. We observe that convection has a different morphology in the inner and the outer part of the convection zone simultaneously such that organized geostrophic convection columns are hidden below a near-surface layer of well-mixed highly chaotic convection. While we focus our attention on the buoyancy-dominated regime, we also demonstrate that conical differential rotation profiles and persistent regular dynamo oscillations can be obtained in the parameter space of the rotation-dominated regime even within this minimal model.
C1 [Simitev, Radostin D.] Univ Glasgow, Sch Math & Stat, Glasgow G12 8QW, Lanark, Scotland.
[Simitev, Radostin D.; Busse, Friedrich H.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Simitev, Radostin D.; Kosovichev, Alexander G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kosovichev, Alexander G.] New Jersey Inst Technol, Newark, NJ 07103 USA.
[Busse, Friedrich H.] Univ Bayreuth, Inst Phys, D-95440 Bayreuth, Germany.
RP Simitev, RD (reprint author), Univ Glasgow, Sch Math & Stat, Glasgow G12 8QW, Lanark, Scotland.
RI Simitev, Radostin/A-4158-2011
OI Simitev, Radostin/0000-0002-2207-5789
FU NASA [NNX14AB70G, NNX09AJ85G]; Leverhulme Trust [RPG-2012-600]
FX This research has been supported by the NASA Grants NNX14AB70G and
NNX09AJ85G and by the Leverhulme Trust Research Project Grant
RPG-2012-600. The hospitality of Stanford University, UCLA, and NASA
Ames Research Center is gratefully acknowledged. R.D.S. enjoyed a period
of study leave granted by the University of Glasgow.
NR 63
TC 4
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2015
VL 810
IS 1
DI 10.1088/0004-637X/810/1/80
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900080
ER
PT J
AU Thomas, S
Belikov, R
Bendek, E
AF Thomas, S.
Belikov, R.
Bendek, E.
TI TECHNIQUES FOR HIGH-CONTRAST IMAGING IN MULTI-STAR SYSTEMS. I.
SUPER-NYQUIST WAVEFRONT CONTROL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: visual; instrumentation: adaptive optics; planet-disk
interactions; planetary systems; planets and satellites: detection
ID DIFFRACTIVE PUPIL
AB Direct imaging of extra-solar planets is now a reality with the deployment and commissioning of the first generation of specialized ground-based instruments (GPI, SPHERE, P1640, and SCExAO). These systems allow of planets 107 times fainter than their host star. For space-based missions (EXCEDE, EXO-C, EXO-S, WFIRST), various teams have demonstrated laboratory contrasts reaching 10(-10) within a few diffraction limits from the star. However, all of these current and future systems are designed to detect faint planets around a single host star, while most non-M-dwarf stars such as Alpha Centauri belong to multi-star systems. Direct imaging around binaries/multiple systems at a level of contrast allowing detection of Earth-like planets is challenging because the region of interest is contaminated by the host star's companion in addition to the host itself. Generally, the light leakage is caused by both diffraction and aberrations in the system. Moreover, the region of interest usually falls outside the correcting zone of the deformable mirror (DM) with respect to the companion. Until now, it has been thought that removing the light of a companion star is too challenging, leading to the exclusion of many binary systems from target lists of direct imaging coronographic missions. In this paper, we will show new techniques for high-contrast imaging of planets around multi-star systems and detail the Super-Nyquist Wavefront Control (SNWC) method, which allows wavefront errors to be controlled beyond the nominal control region of the DM. Our simulations have demonstrated that, with SNWC, raw contrasts of at least 5 x 10(-9) in a 10% bandwidth are possible.
C1 [Thomas, S.; Belikov, R.; Bendek, E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Thomas, S (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
FU National Aeronautics and Space Administration [NAS2-03144]; National
Aeronautics and Space Administration's Ames Research Center under center
investment fund
FX The material is based upon work supported by the National Aeronautics
and Space Administration under Prime Contract Number NAS2-03144 awarded
to the University of California, Santa Cruz, University Affiliated
Research Center. This work was supported in part by the National
Aeronautics and Space Administration's Ames Research Center under a
center investment fund. It was carried out at the NASA Ames Research
Center. Any opinions, findings, and conclusions or recommendations
expressed in this article are those of the authors and do not
necessarily reflect the views of the National Aeronautics and Space
Administration.
NR 17
TC 1
Z9 1
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2015
VL 810
IS 1
AR 81
DI 10.1088/0004-637X/810/1/81
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900081
ER
PT J
AU Veres, P
Corsi, A
Frail, DA
Cenko, SB
Perley, DA
AF Veres, Peter
Corsi, Alessandra
Frail, Dale A.
Cenko, S. Bradley
Perley, Daniel A.
TI EARLY-TIME VLA OBSERVATIONS AND BROADBAND AFTERGLOW ANALYSIS OF THE
FERMI/LAT DETECTED GRB 130907A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general
AB We present multi-wavelength observations of the hyper-energetic gamma-ray burst (GRB) 130907A, a Swift-discovered burst with early radio observations starting at approximate to 4 hr after the gamma-ray trigger. GRB 130907A was also detected by the Fermi/LAT instrument and at late times showed a strong spectral evolution in X-rays. We focus on the early-time radio observations, especially at > 10 GHz, to attempt to identify reverse shock signatures. While our radio follow-up of GRB 130907A ranks among the earliest observations of a GRB with the Karl G. Jansky Very Large Array, we did not see an unambiguous signature of a reverse shock. While a model with both reverse and forward shock can correctly describe the observations, the data is not constraining enough to decide upon the presence of the reverse-shock component. We model the broadband data using a simple forward-shock synchrotron scenario with a transition from a wind environment to a constant density interstellar medium (ISM) in order to account for the observed features. Within the confines of this model, we also derive the underlying physical parameters of the fireball, which are within typical ranges except for the wind density parameter (A(*)), which is higher than those for bursts with wind-ISM transition, but typical for the general population of bursts. We note the importance of early-time radio observations of the afterglow (and of well-sampled light curves) for unambiguously identifying the potential contribution of the reverse shock.
C1 [Veres, Peter] George Washington Univ, Dept Phys, Washington, DC 20052 USA.
[Veres, Peter] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Corsi, Alessandra] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
[Frail, Dale A.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[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.
[Perley, Daniel A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
RP Veres, P (reprint author), George Washington Univ, Dept Phys, 725 21st St NW, Washington, DC 20052 USA.
EM peter.veres@uah.edu
OI Veres, Peter/0000-0002-2149-9846
FU Fermi grant [NNM11AA01A]; OTKA [NN 111016]; NASA-Swift GI program
[13-SWIFT13-0030, 14-SWIFT14-0024]; NASA through Fermi grant
[NNH13ZDA001N]
FX We thank Phil Evans and Bing Zhang for valuable discussions, and the
anonymous referee for useful comments. P.V. acknowledges support from
Fermi grant NNM11AA01A and OTKA NN 111016 grant. A.C. acknowledges
partial support from the NASA-Swift GI program via grants
13-SWIFT13-0030 and 14-SWIFT14-0024. Support for S.B.C. was provided by
NASA through the Fermi grant NNH13ZDA001N. This work made use of data
supplied by the UK Swift Science Data Centre at the University of
Leicester.
NR 0
TC 4
Z9 4
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2015
VL 810
IS 1
AR 31
DI 10.1088/0004-637X/810/1/31
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CS1CT
UT WOS:000361800900031
ER
PT J
AU Walsh, KJE
Camargo, SJ
Vecchi, GA
Daloz, AS
Elsner, J
Emanuel, K
Horn, M
Lim, YK
Roberts, M
Patricola, C
Scoccimarro, E
Sobel, AH
Strazzo, S
Villarini, G
Wehner, M
Zhao, M
Kossin, JP
LaRow, T
Oouchi, K
Schubert, S
Wang, H
Bacmeister, J
Chang, P
Chauvin, F
Jablonowski, C
Kumar, A
Murakami, H
Ose, T
Reed, KA
Saravanan, R
Yamada, Y
Zarzycki, CM
Vidale, PL
Jonas, JA
Henderson, N
AF Walsh, Kevin J. E.
Camargo, Suzana J.
Vecchi, Gabriel A.
Daloz, Anne Sophie
Elsner, James
Emanuel, Kerry
Horn, Michael
Lim, Young-Kwon
Roberts, Malcolm
Patricola, Christina
Scoccimarro, Enrico
Sobel, Adam H.
Strazzo, Sarah
Villarini, Gabriele
Wehner, Michael
Zhao, Ming
Kossin, James P.
LaRow, Tim
Oouchi, Kazuyoshi
Schubert, Siegfried
Wang, Hui
Bacmeister, Julio
Chang, Ping
Chauvin, Fabrice
Jablonowski, Christiane
Kumar, Arun
Murakami, Hiroyuki
Ose, Tomoaki
Reed, Kevin A.
Saravanan, Ramalingam
Yamada, Yohei
Zarzycki, Colin M.
Vidale, Pier Luigi
Jonas, Jeffrey A.
Henderson, Naomi
TI HURRICANES AND CLIMATE: THE U.S. CLIVAR WORKING GROUP ON HURRICANES (vol
96, pg 997, 2015)
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Correction
C1 [Walsh, Kevin J. E.; Horn, Michael] Univ Melbourne, Parkville, Vic 3010, Australia.
[Camargo, Suzana J.; Sobel, Adam H.; Henderson, Naomi] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Vecchi, Gabriel A.; Zhao, Ming; Murakami, Hiroyuki] Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Daloz, Anne Sophie] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
[Elsner, James; Strazzo, Sarah; LaRow, Tim] Florida State Univ, Tallahassee, FL 32306 USA.
[Emanuel, Kerry] MIT, Cambridge, MA 02139 USA.
[Lim, Young-Kwon; Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Lim, Young-Kwon] Goddard Earth Sci Technol & Res, Greenbelt, MD USA.
[Lim, Young-Kwon] IM Syst Grp, Greenbelt, MD USA.
[Roberts, Malcolm] Met Off, Exeter, Devon, England.
[Patricola, Christina; Chang, Ping; Saravanan, Ramalingam] Texas A&M Univ, College Stn, TX USA.
[Scoccimarro, Enrico] Ist Nazl Geofis & Vulcanol, Bologna, Italy.
[Scoccimarro, Enrico] Ctr Euromediterraneo Cambiamenti Climat, Bologna, Italy.
[Villarini, Gabriele] Univ Iowa, Iowa City, IA USA.
[Wehner, Michael] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Kossin, James P.] NOAA, NCDC, Asheville, NC USA.
[Oouchi, Kazuyoshi; Yamada, Yohei] JAMSTEC, Yokohama, Kanagawa, Japan.
[Wang, Hui; Kumar, Arun] NOAA, NCEP, College Pk, MD USA.
[Bacmeister, Julio; Reed, Kevin A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Chauvin, Fabrice] Meteo France, Toulouse, France.
[Jablonowski, Christiane; Zarzycki, Colin M.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Ose, Tomoaki] Japan Meteorol Agcy, Meteorol Res Inst, Tsukuba, Ibaraki, Japan.
[Vidale, Pier Luigi] Univ Reading, Reading, Berks, England.
[Jonas, Jeffrey A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Jonas, Jeffrey A.] Columbia Univ, New York, NY USA.
RP Walsh, KJE (reprint author), Univ Melbourne, Sch Earth Sci, Parkville, Vic 3010, Australia.
EM kevin.walsh@unimelb.edu.au
RI Vecchi, Gabriel/A-2413-2008; Camargo, Suzana/C-6106-2009; Zhao,
Ming/C-6928-2014; Jablonowski, Christiane/I-9068-2012; Kossin,
James/C-2022-2016; Chang, Ping /A-1642-2013; Villarini,
Gabriele/F-8069-2016; Sobel, Adam/K-4014-2015; Zarzycki,
Colin/E-5691-2014; Patricola, Christina/L-9902-2016
OI Vecchi, Gabriel/0000-0002-5085-224X; Walsh, Kevin/0000-0002-1860-510X;
Camargo, Suzana/0000-0002-0802-5160; Jablonowski,
Christiane/0000-0003-0407-0092; Kossin, James/0000-0003-0461-9794;
Chang, Ping /0000-0002-9085-0759; Villarini,
Gabriele/0000-0001-9566-2370; Sobel, Adam/0000-0003-3602-0567;
Patricola, Christina/0000-0002-3387-0307
NR 1
TC 0
Z9 0
U1 0
U2 10
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD SEP
PY 2015
VL 96
IS 9
BP 1440
EP 1440
DI 10.1175/BAMS-D-15-00232.1
PG 1
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CS6QV
UT WOS:000362206900001
ER
PT J
AU Massa, GD
Norrie, J
AF Massa, Gioia D.
Norrie, Jeff
TI LEDs Electrifying Horticultural Science: Proceedings from the 2014
Colloquium and Workshop
SO HORTSCIENCE
LA English
DT Article
DE commercial technology; controlled environment; light emitting diode;
light quality
ID LIGHT
C1 [Massa, Gioia D.] NASA, UB A, Kennedy Space Ctr, FL 32899 USA.
[Norrie, Jeff] Acad Seaplants Ltd, Dartmouth, NS B3B 1X8, Canada.
RP Massa, GD (reprint author), NASA, UB A, Kennedy Space Ctr, FL 32899 USA.
EM gioia.massa@nasa.gov
NR 10
TC 0
Z9 0
U1 6
U2 6
PU AMER SOC HORTICULTURAL SCIENCE
PI ALEXANDRIA
PA 113 S WEST ST, STE 200, ALEXANDRIA, VA 22314-2851 USA
SN 0018-5345
EI 2327-9834
J9 HORTSCIENCE
JI Hortscience
PD SEP
PY 2015
VL 50
IS 9
BP 1272
EP 1273
PG 2
WC Horticulture
SC Agriculture
GA CS8BD
UT WOS:000362309800001
ER
PT J
AU Xue, M
Zelinski, S
AF Xue, Min
Zelinski, Shannon
TI Integrated Arrival- and Departure-Schedule Optimization Under
Uncertainty
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID STOCHASTIC DIFFERENTIAL-EQUATIONS; PROBABILISTIC COLLOCATION METHOD;
POLYNOMIAL CHAOS; MODELS
AB In terminal airspace, integrating arrivals and departures with shared waypoints provides the potential of improving operational efficiency by allowing direct routes when possible. Incorporating stochastic evaluation as a postanalysis process of deterministic optimization and imposing a safety buffer in deterministic optimization are two ways to learn and alleviate the impact of uncertainty and to avoid unexpected outcomes. This work presents a third and direct way to take uncertainty into consideration during the optimization. The impact of uncertainty was incorporated into cost evaluations when searching for the optimal solutions. The controller intervention count was computed using a heuristic model and served as another stochastic cost in addition to total delay. Costs under uncertainty were evaluated using MonteCarlo simulations. The Pareto fronts that contained a set of solutions were identified, and the tradeoff between delays and controller intervention count was shown. Solutions that shared similar delays but had different intervention counts were investigated. The results showed that optimization under uncertainty could identify compromise solutions on Pareto fonts, which is better than deterministic optimization with extra safety buffers. It helps decision makers reduce controller intervention while achieving low delays.
C1 [Xue, Min] Univ Calif Santa Cruz, Univ Affiliated Res Ctr, Moffett Field, CA 94035 USA.
[Zelinski, Shannon] NASA, Ames Res Ctr, Aerosp High Dens Operat Branch, Moffett Field, CA 94035 USA.
RP Xue, M (reprint author), Univ Calif Santa Cruz, Univ Affiliated Res Ctr, Mail Stop 210-8, Moffett Field, CA 94035 USA.
NR 14
TC 0
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 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD SEP-OCT
PY 2015
VL 52
IS 5
BP 1437
EP 1443
DI 10.2514/1.C032957
PG 7
WC Engineering, Aerospace
SC Engineering
GA CS4JI
UT WOS:000362041700007
ER
PT J
AU Pak, CG
Truong, S
AF Pak, Chan-gi
Truong, Samson
TI Creating a Test-Validated Finite-Element Model of the X-56A Aircraft
Structure
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID BANG-BIG-CRUNCH; OPTIMIZATION
AB Small modeling errors in a finite-element model will eventually induce errors in the structural flexibility and mass, thus propagating into unpredictable errors in the unsteady aerodynamics and the control law design. One of the primary objectives of the X-56A Multi-Utility Technology Testbed aircraft is the flight demonstration of active flutter suppression and, therefore, in this study, the identification of the primary and secondary modes for the structural model tuning based on the flutter analysis of the X-56A aircraft. The ground-vibration test-validated structural dynamic finite-element model of the X-56A aircraft is created in this study. The structural dynamic finite-element model of the X-56A aircraft is improved using a model-tuning tool. In this study, two different weight configurations of the X-56A aircraft have been improved in a single optimization run. Frequency and the cross-orthogonality (mode shape) matrix were the primary focus for improvement, whereas other properties such as c.g. location, total weight, and off-diagonal terms of the mass orthogonality matrix were used as constraints. The end result was an improved structural dynamic finite-element model configuration for the X-56A aircraft. Improved frequencies and mode shapes in this study increased average flutter speeds of the X-56A aircraft by 7.6% compared to the baseline model.
C1 [Pak, Chan-gi; Truong, Samson] NASA, Armstrong Flight Res Ctr, Aerostruct Branch, Edwards AFB, CA 93523 USA.
RP Pak, CG (reprint author), NASA, Armstrong Flight Res Ctr, Aerostruct Branch, POB 273,Mail Stop 48201A, Edwards AFB, CA 93523 USA.
FU Aero Science Project
FX The work presented in this paper was funded by the Aero Science Project
under the ARMD Fundamental Aeronautics Program. The project managers at
NASA AFRC were Mark Davis and Robert Navarro. The authors also thank
Jeff Beranek at Lockheed Martin Skunk Works for his support in providing
the finite-element models and the ground-vibration test data during this
research. Finally, thanks to Pete Flick at the U.S. Air Force Research
Laboratory for providing the flight hardware and test data to NASA.
NR 23
TC 0
Z9 0
U1 1
U2 2
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD SEP-OCT
PY 2015
VL 52
IS 5
BP 1644
EP 1667
DI 10.2514/1.C033043
PG 24
WC Engineering, Aerospace
SC Engineering
GA CS4JI
UT WOS:000362041700024
ER
PT J
AU Thompson, PA
Bonham, P
Thomson, P
Rochester, W
Doblin, MA
Waite, AM
Richardson, A
Rousseaux, CS
AF Thompson, Peter A.
Bonham, Pru
Thomson, Paul
Rochester, Wayne
Doblin, Martina A.
Waite, Anya M.
Richardson, Anthony
Rousseaux, Cecile S.
TI Climate variability drives plankton community composition changes: the
2010-2011 El Nino to La Nina transition around Australia
SO JOURNAL OF PLANKTON RESEARCH
LA English
DT Article
DE nutrients; phytoplankton; zooplankton; ENSO; climate
ID COASTAL UPWELLING SYSTEM; LEEUWIN CURRENT EDDIES; NORTH-WEST-CAPE;
INDIAN-OCEAN; SOUTHEAST AUSTRALIA; INTERANNUAL VARIATIONS; EQUATORIAL
PACIFIC; SUBTROPICAL FRONT; EASTERN AUSTRALIA; OBSERVING SYSTEM
AB The strong La Nina of 2010-2011 provided an opportunity to investigate the ecological impacts of El Nino-Southern Oscillation on coastal plankton communities using the nine national reference stations around Australia. Based on remote sensing and across the entire Australian region 2011 (La Nina) was only modestly different from 2010 (El Nino) with the average temperature declining 0.2%, surface chlorophyll a up 3% and modelled primary production down 14%. Other changes included a poleward shift in Prochlorococcus and Synechococcus. Along the east coast, there was a reduction in salinity, increase in nutrients, Chlorophytes and Prasinophytes (taxa with chlorophyll b, neoxanthin and prasinoxanthin). The southwest region had a rise in the proportion of 19-hexoyloxyfucoxanthin; possibly cocco-lithophorids in eddies of the Leeuwin Current and along the sub-tropical front. Pennate diatoms increased, Ceratium spp. decreased and Scrippsiella spp. increased in 2011. Zooplankton biomass declined significantly in 2011. There was a reduction in the abundance of Calocalanus pavo and Temora turbinata and increases in Clausocalanus farrani, Oncaea scottodicarloi and Macrosetella gracilis in 2011. The changes in the plankton community during the strong La Nina of 2011 suggest that this climatic oscillation exacerbates the tropicalization of Australia.
C1 [Thompson, Peter A.; Bonham, Pru] CSIRO, Oceans & Atmosphere Flagship, Hobart, Tas 7001, Australia.
[Thomson, Paul; Waite, Anya M.] Univ Western Australia, Sch Environm Syst Engn, Crawley, WA 6009, Australia.
[Rochester, Wayne; Richardson, Anthony] CSIRO, Ecosci Precinct, Oceans & Atmosphere Flagship, Brisbane, Qld 4001, Australia.
[Doblin, Martina A.] Univ Technol Sydney, Plant Funct Biol & Climate Change Cluster, Environm Sci, Sydney, NSW 2007, Australia.
[Rousseaux, Cecile S.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Rousseaux, Cecile S.] Univ Space Res Assoc, Columbia, MD USA.
RP Thompson, PA (reprint author), CSIRO, Oceans & Atmosphere Flagship, GPO BOX 1538, Hobart, Tas 7001, Australia.
EM peter.a.thompson@csiro.au
RI Thompson, Peter/A-2361-2012; Waite, Anya/A-5492-2015; Rousseaux,
Cecile/E-8811-2012;
OI Thompson, Peter/0000-0002-9504-5433; Waite, Anya/0000-0003-2965-0296;
Rousseaux, Cecile/0000-0002-3022-2988; Doblin,
Martina/0000-0001-8750-3433
FU CSIRO Oceans and Atmosphere; NASA Modeling, Analysis, and Prediction
(MAP) Program; PACE Program
FX P.A.T. was supported by CSIRO Oceans and Atmosphere. Funding to support
the contribution of C.S.R. was provided by the NASA Modeling, Analysis,
and Prediction (MAP) and PACE Programs. The authors acknowledge the
facilities, and the scientific and technical assistance of the
Australian Microscopy & Microanalysis Research Facility at the Centre
for Microscopy, Characterisation and Analysis at the University of
Western Australia, a facility funded by the University, State and
Commonwealth Governments.
NR 99
TC 2
Z9 2
U1 8
U2 39
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0142-7873
EI 1464-3774
J9 J PLANKTON RES
JI J. Plankton Res.
PD SEP-OCT
PY 2015
VL 37
IS 5
BP 966
EP 984
DI 10.1093/plankt/fbv069
PG 19
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA CS3RY
UT WOS:000361993700011
ER
PT J
AU Driscoll, PE
Barnes, R
AF Driscoll, P. E.
Barnes, R.
TI Tidal Heating of Earth-like Exoplanets around M Stars: Thermal,
Magnetic, and Orbital Evolutions
SO ASTROBIOLOGY
LA English
DT Article
ID SOLAR-SYSTEM; MANTLE CONVECTION; HABITABLE ZONES; ICY SATELLITES;
SUPER-EARTHS; OCEAN TIDES; CORE; DISSIPATION; PLANETS; DRIVEN
AB The internal thermal and magnetic evolution of rocky exoplanets is critical to their habitability. We focus on the thermal-orbital evolution of Earth-mass planets around low-mass M stars whose radiative habitable zone overlaps with the tidal zone, where tidal dissipation is expected to be a significant heat source in the interior. We develop a thermal-orbital evolution model calibrated to Earth that couples tidal dissipation, with a temperature-dependent Maxwell rheology, to orbital circularization and migration. We illustrate thermal-orbital steady states where surface heat flow is balanced by tidal dissipation and cooling can be stalled for billions of years until circularization occurs. Orbital energy dissipated as tidal heat in the interior drives both inward migration and circularization, with a circularization time that is inversely proportional to the dissipation rate. We identify a peak in the internal dissipation rate as the mantle passes through a viscoelastic state at mantle temperatures near 1800K. Planets orbiting a 0.1 solar-mass star within 0.07 AU circularize before 10 Gyr, independent of initial eccentricity. Once circular, these planets cool monotonically and maintain dynamos similar to that of Earth. Planets forced into eccentric orbits can experience a super-cooling of the core and rapid core solidification, inhibiting dynamo action for planets in the habitable zone. We find that tidal heating is insignificant in the habitable zone around 0.45 (or larger) solar-mass stars because tidal dissipation is a stronger function of orbital distance than stellar mass, and the habitable zone is farther from larger stars. Suppression of the planetary magnetic field exposes the atmosphere to stellar wind erosion and the surface to harmful radiation. In addition to weak magnetic fields, massive melt eruption rates and prolonged magma oceans may render eccentric planets in the habitable zone of low-mass stars inhospitable for life. Key Words: Tidal dissipationThermal historyPlanetary interiorsMagnetic field. Astrobiology 15, 739-760.
C1 [Driscoll, P. E.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
NASA, Astrobiol Inst, Virtual Planetary Lab, Lead Team, Washington, DC USA.
RP Driscoll, PE (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM ped13@uw.edu
FU National Aeronautics and Space Administration through the NASA
Astrobiology Institute [NNH12ZDA002C, NNA13AA93A]
FX The authors thank W. Henning and T. Hurford for helpful discussions and
two anonymous reviewers for valuable feedback. This work was performed
as part of the NASA Astrobiology Institute's Virtual Planetary
Laboratory, supported by the National Aeronautics and Space
Administration through the NASA Astrobiology Institute under
solicitation NNH12ZDA002C and Cooperative Agreement Number NNA13AA93A.
NR 73
TC 11
Z9 11
U1 0
U2 6
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
EI 1557-8070
J9 ASTROBIOLOGY
JI Astrobiology
PD SEP 1
PY 2015
VL 15
IS 9
BP 739
EP 760
DI 10.1089/ast.2015.1325
PG 22
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA CR7IQ
UT WOS:000361523200004
PM 26393398
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 Reply to "Comments on 'Describing the Shape of Raindrop Size
Distributions Using Uncorrelated Raindrop Mass Spectrum Parameters"'
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Letter
DE Rainfall
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, Baltimore, MD 21228 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
NR 7
TC 0
Z9 0
U1 1
U2 1
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 SEP
PY 2015
VL 54
IS 9
BP 1977
EP 1982
DI 10.1175/JAMC-D-15-0058.1
PG 6
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CS1BP
UT WOS:000361797800011
ER
PT J
AU Plante, I
Cucinotta, FA
AF Plante, I.
Cucinotta, F. A.
TI BINARY-ENCOUNTER-BETHE IONISATION CROSS SECTIONS FOR SIMULATION OF DNA
DAMAGE BY THE DIRECT EFFECT OF IONISING RADIATION
SO RADIATION PROTECTION DOSIMETRY
LA English
DT Article; Proceedings Paper
CT 16th International Symposium on Microdosimetry (MICROS)
CY OCT 20-25, 2013
CL Trevisto, ITALY
SP INFN, Lab Nazl Legnaro, NASA, Johnson Space Ctr, Univ Nevada, Houston & Hlth Phys & Diagnost Sci Dept, Int Commiss Radiat Units & Measurements, Univ Oxford, Oxford Inst Radiat Oncol
ID MODEL
AB DNA damage is of crucial importance in the understanding of the effects of ionising radiation. To refine existing DNA damage models, an approach using the Binary-Encounter-Bethe (BEB) cross sections was developed. The differential cross sections for ionisation of the molecular orbitals of the DNA bases, sugars and phosphates are calculated using the electron binding energy, the mean kinetic energy and the occupancy number of each orbital as parameters. The resulting cross section has an analytic form which is quite convenient to use for Monte-Carlo codes that randomly sample the energy loss occurring during an ionisation event. We also describe an algorithm to simulate the interactions of electrons with DNA in the radiation transport code RITRACKS using the integrated BEB cross section for the bases, sugar and phosphates.
C1 [Plante, I.] NASA, Lyndon B Johnson Space Ctr, Wyle Sci Technol & Engn, Houston, TX 77058 USA.
[Cucinotta, F. A.] Univ Nevada, Hlth Phys & Diagnost Sci, Las Vegas, NV 89154 USA.
RP Plante, I (reprint author), NASA, Lyndon B Johnson Space Ctr, Wyle Sci Technol & Engn, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM ianik.plante-1@nasa.gov
FU National Aeronautics and Space Administration (NASA) [NAS9-02078]
FX Funding for this project was provided through the National Aeronautics
and Space Administration (NASA contract number NAS9-02078).
NR 9
TC 0
Z9 0
U1 1
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0144-8420
EI 1742-3406
J9 RADIAT PROT DOSIM
JI Radiat. Prot. Dosim.
PD SEP
PY 2015
VL 166
IS 1-4
BP 19
EP 23
DI 10.1093/rpd/ncv143
PG 5
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA CS1EX
UT WOS:000361806600005
PM 25870431
ER
PT J
AU Plante, I
Cucinotta, FA
AF Plante, I.
Cucinotta, F. A.
TI SIMULATION OF THE RADIOLYSIS OF WATER USING GREEN'S FUNCTIONS OF THE
DIFFUSION EQUATION
SO RADIATION PROTECTION DOSIMETRY
LA English
DT Article; Proceedings Paper
CT 16th International Symposium on Microdosimetry (MICROS)
CY OCT 20-25, 2013
CL Trevisto, ITALY
SP INFN, Lab Nazl Legnaro, NASA, Johnson Space Ctr, Univ Nevada, Houston & Hlth Phys & Diagnost Sci Dept, Int Commiss Radiat Units & Measurements, Univ Oxford, Oxford Inst Radiat Oncol
ID MONTE-CARLO; CHEMISTRY; ELECTRON; KINETICS; SPACE; STATE; TIME
AB Radiation chemistry is of fundamental importance in the understanding of the effects of ionising radiation, notably with regard to DNA damage by indirect effect (e.g. damage by center dot OH radicals created by the radiolysis of water). In the recent years, Green's functions of the diffusion equation (GFDEs) have been used extensively in biochemistry, notably to simulate biochemical networks in time and space. In the present work, an approach based on the GFDE will be used to refine existing models on the indirect effect of ionising radiation on DNA. As a starting point, the code RITRACKS (relativistic ion tracks) will be used to simulate the radiation track structure and calculate the position of all radiolytic species formed during irradiation. The chemical reactions between these radiolytic species and with DNA will be done by using an efficient Monte Carlo sampling algorithm for the GFDE of reversible reactions with an intermediate state that has been developed recently. These simulations should help the understanding of the contribution of the indirect effect in the formation of DNA damage, particularly with regards to the formation of double-strand breaks.
C1 [Plante, I.] NASA, Lyndon B Johnson Space Ctr, Wyle Sci Technol & Engn, Houston, TX 77058 USA.
[Cucinotta, F. A.] Univ Nevada, Hlth Phys & Diagnost Sci, Las Vegas, NV 89154 USA.
RP Plante, I (reprint author), NASA, Lyndon B Johnson Space Ctr, Wyle Sci Technol & Engn, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM ianik.plante-1@nasa.gov
FU National Aeronautics and Space Administration (NASA) [NAS9-02078]
FX Funding for this project was provided through the National Aeronautics
and Space Administration (NASA) contract number NAS9-02078.
NR 16
TC 1
Z9 1
U1 3
U2 7
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0144-8420
EI 1742-3406
J9 RADIAT PROT DOSIM
JI Radiat. Prot. Dosim.
PD SEP
PY 2015
VL 166
IS 1-4
BP 24
EP 28
DI 10.1093/rpd/ncv179
PG 5
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA CS1EX
UT WOS:000361806600006
PM 25897139
ER
PT J
AU Guo, JN
Zeitlin, C
Wimmer-Schweingruber, RF
Hassler, DM
Ehresmann, B
Kohler, J
Bohm, E
Bottcher, S
Brinza, D
Burmeister, S
Cucinotta, F
Martin, C
Posner, A
Rafkin, S
Reitz, G
AF Guo, Jingnan
Zeitlin, Cary
Wimmer-Schweingruber, Robert F.
Hassler, Donald M.
Ehresmann, Bent
Koehler, Jan
Boehm, Eckart
Boettcher, Stephan
Brinza, David
Burmeister, Soenke
Cucinotta, Francis
Martin, Cesar
Posner, Arik
Rafkin, Scot
Reitz, Guenther
TI MSL-RAD RADIATION ENVIRONMENT MEASUREMENTS
SO RADIATION PROTECTION DOSIMETRY
LA English
DT Article; Proceedings Paper
CT 16th International Symposium on Microdosimetry (MICROS)
CY OCT 20-25, 2013
CL Trevisto, ITALY
SP INFN, Lab Nazl Legnaro, NASA, Johnson Space Ctr, Univ Nevada, Houston & Hlth Phys & Diagnost Sci Dept, Int Commiss Radiat Units & Measurements, Univ Oxford, Oxford Inst Radiat Oncol
ID ENERGETIC PARTICLE RADIATION; ASSESSMENT DETECTOR; MARS; SURFACE; SUITE
AB In this study, results are presented from the on-board radiation assessment detector (RAD) of Mars Science Laboratory (MSL). RAD is designed to measure the energetic particle radiation environment, which consists of galactic cosmic rays (GCRs) and solar energetic particles (SEPs) as well as secondary particles created by nuclear interactions of primary particles in the shielding (during cruise) or Martian soil and atmosphere (surface measurements). During the cruise, RAD collected data on space radiation from inside the craft, thus allowing for a reasonable estimation of what a human crew travelling to/from Mars might be exposed to. On the surface of Mars, RAD is shielded by the atmosphere (from above) and the planet itself (from below). RAD measures the first detailed radiation data from the surface of another planet, and they are highly relevant for planning future crewed missions. The results for radiation dose and dose equivalent (a quantity most directly related to human health risk) are presented during the cruise phase, as well as on the Martian surface. Dose and dose equivalent are dominated by the continuous GCR radiation, but several SEP events were also detected and are discussed here.
C1 [Guo, Jingnan; Wimmer-Schweingruber, Robert F.; Koehler, Jan; Boehm, Eckart; Boettcher, Stephan; Burmeister, Soenke; Martin, Cesar] Univ Kiel, Kiel, Germany.
[Zeitlin, Cary] Southwest Res Inst, Durham, NH USA.
[Hassler, Donald M.; Ehresmann, Bent; Rafkin, Scot] Southwest Res Inst, Boulder, CO USA.
[Brinza, David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cucinotta, Francis] UNLV, Las Vegas, NV USA.
[Posner, Arik] NASA Headquarters, Washington, DC USA.
[Reitz, Guenther] DLR, Cologne, Germany.
RP Guo, JN (reprint author), Univ Kiel, Kiel, Germany.
EM guo@physik.uni-kiel.de
FU National Aeronautics and Space Administration (NASA) under JPL
[1273039]; DLR; DLR's Space Administration [50QM0501, 50QM1201]
FX RAD is supported by the National Aeronautics and Space Administration
(NASA) under JPL subcontract 1273039 to the Southwest Research Institute
and by DLR and DLR's Space Administration, grant numbers 50QM0501 and
50QM1201, to the Christian Albrechts University in Kiel, Germany. Part
of this research was carried out at JPL under a contact with NASA.
NR 13
TC 0
Z9 0
U1 5
U2 12
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0144-8420
EI 1742-3406
J9 RADIAT PROT DOSIM
JI Radiat. Prot. Dosim.
PD SEP
PY 2015
VL 166
IS 1-4
BP 290
EP 294
DI 10.1093/rpd/ncv297
PG 5
WC Environmental Sciences; Public, Environmental & Occupational Health;
Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical
Imaging
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
GA CS1EX
UT WOS:000361806600059
PM 25969529
ER
PT J
AU Brampton, CJ
Wu, KC
Kim, HA
AF Brampton, Christopher J.
Wu, K. Chauncey
Kim, H. Alicia
TI New optimization method for steered fiber composites using the level set
method
SO STRUCTURAL AND MULTIDISCIPLINARY OPTIMIZATION
LA English
DT Article
DE Fiber-matrix composite; Fibre path optimization; Level set method;
Compliance minimization
ID STRUCTURAL OPTIMIZATION; LAMINATION PARAMETERS; TOPOLOGY OPTIMIZATION;
ORTHOTROPIC MATERIALS; GENETIC ALGORITHM; DESIGN; ORIENTATIONS;
CAPACITY; SHELL; HOLE
AB Advanced fiber placement (AFP) composite manufacturing technology offers a means to tailor composite fibers for complex loading environments and significantly improve the overall structural efficiency. This paper introduces a new method to optimize the continuously varying fiber paths for AFP using a level set method. The paths of the fibers are defined by constant level set function values, describing a series of continuous equally spaced fiber paths. The sensitivity of the structural compliance to a change in level set function definition of the fiber path is derived. The sensitivities are used to optimize the level set defined fiber paths to minimize structural compliance, while maintaining the continuous fiber paths and producing a solution that can be manufactured using AFP. The optimization method is demonstrated in three numerical studies.
C1 [Brampton, Christopher J.; Kim, H. Alicia] Univ Bath, Dept Mech Engn, Bath BA2 7AY, Avon, England.
[Wu, K. Chauncey] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
RP Brampton, CJ (reprint author), Univ Bath, Dept Mech Engn, Bath BA2 7AY, Avon, England.
EM cjb31@bath.ac.uk
OI Kim, Hyunsun Alicia/0000-0002-5629-2466
FU NASA's Fixed Wing Project under the Fundamental Aeronautics Program
FX This work was funded by NASA's Fixed Wing Project under the Fundamental
Aeronautics Program.
NR 45
TC 1
Z9 1
U1 3
U2 12
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 SEP
PY 2015
VL 52
IS 3
BP 493
EP 505
DI 10.1007/s00158-015-1256-6
PG 13
WC Computer Science, Interdisciplinary Applications; Engineering,
Multidisciplinary; Mechanics
SC Computer Science; Engineering; Mechanics
GA CR7YU
UT WOS:000361568900005
ER
PT J
AU Cosentino, RG
Simon, A
Morales-Juberias, R
Sayanagi, KM
AF Cosentino, R. G.
Simon, A.
Morales-Juberias, R.
Sayanagi, K. M.
TI OBSERVATIONS AND NUMERICAL MODELING OF THE JOVIAN RIBBON
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: general;
planets and satellites: physical evolution
ID JUPITERS ATMOSPHERE; CASSINI; IMAGES; SATURN; WAVES; SPOT
AB Multiple wavelength observations made by the Hubble Space Telescope in early 2007 show the presence of a wavy, high-contrast feature in Jupiter's atmosphere near 30 degrees N. The "Jovian Ribbon," best seen at 410 nm, irregularly undulates in latitude and is time-variable in appearance. A meridional intensity gradient algorithm was applied to the observations to track the Ribbon's contour. Spectral analysis of the contour revealed that the Ribbon's structure is a combination of several wavenumbers ranging from k = 8-40. The Ribbon is a dynamic structure that has been observed to have spectral power for dominant wavenumbers which vary over a time period of one month. The presence of the Ribbon correlates with periods when the velocity of the westward jet at the same location is highest. We conducted numerical simulations to investigate the stability of westward jets of varying speed, vertical shear, and background static stability to different perturbations. A Ribbon-like morphology was best reproduced with a 35 ms(-1) westward jet that decreases in amplitude for pressures greater than 700 hPa and a background static stability of N = 0.005 s(-1) perturbed by heat pulses constrained to latitudes south of 30 degrees N. Additionally, the simulated feature had wavenumbers that qualitatively matched observations and evolved throughout the simulation reproducing the Jovian Ribbon's dynamic structure.
C1 [Cosentino, R. G.; Morales-Juberias, R.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA.
[Simon, A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Sayanagi, K. M.] Hampton Univ, Hampton, VA 23668 USA.
RP Cosentino, RG (reprint author), New Mexico Inst Min & Technol, Socorro, NM 87801 USA.
EM rickcos@nmt.edu.com
RI Simon, Amy/C-8020-2012
OI Simon, Amy/0000-0003-4641-6186
FU Association of Universities for Research in Astronomy, Inc., under NASA
[NAS5-26555]; NASA PATM [NNX14AH47G]; NASA OPR [NNX12AR38G]
FX This work was based on observations made with the NASA/ESA Hubble Space
Telescope under programs GO/DD 5313, 5642, 6009, 6452, 7616, 8148, 8405,
10782, 11096, 11102, 11310, and 11498, publicly available through the
Mikulski Archive for Space Telescopes. The Space Telescope Science
Institute is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS5-26555. All Voyager data are
available through the Planetary Data System. Computational resources
were provided by New Mexico Institute of Mining and Technology and by
Computational and Information Systems Laboratory at National Center for
Atmospheric Research. Yellowstone: IBM iDataPlex System. Boulder, CO.
This work was partially supported by NASA PATM grant # NNX14AH47G to
A.S. K.M.S. was supported in part by NASA OPR grant # NNX12AR38G.
NR 18
TC 1
Z9 1
U1 0
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 SEP 1
PY 2015
VL 810
IS 1
AR L10
DI 10.1088/2041-8205/810/1/L10
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ6LJ
UT WOS:000360715600010
ER
PT J
AU Sahai, R
Patel, NA
AF Sahai, R.
Patel, N. A.
TI AN EXTREME HIGH-VELOCITY BIPOLAR OUTFLOW IN THE PRE-PLANETARY NEBULA
IRAS 08005-2356
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; circumstellar matter; planetary nebulae:
individual (IRAS08005-2356); stars: AGB and post-AGB; stars: mass-loss;
stars: winds, outflows
ID YOUNG PLANETARY-NEBULAE; MORPHOLOGICAL CLASSIFICATION-SYSTEM; POST-AGB
STARS; PROTOPLANETARY NEBULA; EVOLVED STARS; LARGE GRAINS; HD 101584;
SPECTROSCOPY; CANDIDATES; ENVELOPE
AB We report interferometric mapping of the bipolar pre-planetary nebula IRAS 08005-2356 (I 08005) with an angular resolution of similar to 1 ''-5 '', using the Submillimeter Array, in the (CO)-C-12 J = 2-1, 3-2, (CO)-C-13 J = 2-1, and SiO J = 5-4 (v = 0) lines. Single-dish observations, using the SMT 10 m, were made in these lines as well as in the CO J = 4-3 and SiO J = 6-5 (v = 0) lines. The line profiles are very broad, showing the presence of a massive (>0.1 M-circle dot), extreme high velocity outflow (V similar to 200 km s(-1)) directed along the nebular symmetry axis derived from the Hubble Space Telescope imaging of this object. The outflow's scalar momentum far exceeds that available from radiation pressure of the central post-AGB star, and it may be launched from an accretion disk around a main-sequence companion. We provide indirect evidence for such a disk from its previously published, broad Ha emission profile, which we propose results from Ly beta emission generated in the disk followed by Raman-scattering in the innermost regions of a fast, neutral wind.
C1 [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Patel, N. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA.
EM raghvendra.sahai@jpl.nasa.gov
FU Smithsonian Institution; Academia Sinica
FX The SMA 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.
NR 30
TC 1
Z9 1
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 SEP 1
PY 2015
VL 810
IS 1
AR L8
DI 10.1088/2041-8205/810/1/L8
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ6LJ
UT WOS:000360715600008
ER
PT J
AU Schwerdt, HN
Miranda, FA
Chae, J
AF Schwerdt, Helen N.
Miranda, Felix A.
Chae, Junseok
TI Wireless Fully Passive Multichannel Recording of Neuropotentials Using
Photo-Activated RF Backscattering Methods
SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES
LA English
DT Article
DE Backscattering; brain-machine interfaces (BMIs); RF identification
(RFID); wireless passive neural recording
ID INSECT TRACKING; HARMONIC RADAR; SENSOR; TISSUE
AB Fully passive RF backscattering for wireless monitoring of neuropotentials, electrical activity generated by neurons, is a promising recording technique that may subdue some of the safety restraints observed in traditional active or passive recording schemes. The fully passive device operates without power supply or regulating elements and exhibits a highly simplified implant circuit topology. However, a critical challenge is its current limitation to single channel recording. Here, a method of integrating multiple channels onto the fully passive system is demonstrated that preserves its fully passive qualities and a single shared antenna. Multichannel recording is implemented by introducing photo-selective and photo-sensitive switches to individual channel electrodes to control the activation of individual recording operations via an external multi-band light source. These multi-modal wireless processes are simulated and implemented on Pyrex substrates that demonstrate recording of emulated neuropotential signals as low as V-m similar to 0.7 mV(pp) with at least 10-dB channel isolation as tested in air.
C1 [Schwerdt, Helen N.; Chae, Junseok] Arizona State Univ, Sch Elect Comp & Energy Engn, Tempe, AZ 85287 USA.
[Miranda, Felix A.] NASA, Glenn Res Ctr, Adv High Frequency Branch LCF, Cleveland, OH 44135 USA.
RP Schwerdt, HN (reprint author), MIT, Koch Inst Integrat Canc Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM schwerdt@mit.edu
NR 21
TC 0
Z9 0
U1 2
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9480
EI 1557-9670
J9 IEEE T MICROW THEORY
JI IEEE Trans. Microw. Theory Tech.
PD SEP
PY 2015
VL 63
IS 9
BP 2965
EP 2970
DI 10.1109/TMTT.2015.2460746
PG 6
WC Engineering, Electrical & Electronic
SC Engineering
GA CR3OL
UT WOS:000361242500028
ER
PT J
AU Garrett, HB
Whittlesey, AC
AF Garrett, Henry B.
Whittlesey, Albert C.
TI Special Issue on Spacecraft Charging Technology
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Editorial Material
C1 [Garrett, Henry B.; Whittlesey, Albert C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Garrett, HB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 0
TC 0
Z9 0
U1 2
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
EI 1939-9375
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD SEP
PY 2015
VL 43
IS 9
SI SI
BP 2775
EP 2775
DI 10.1109/TPS.2015.2466837
PN 1
PG 1
WC Physics, Fluids & Plasmas
SC Physics
GA CR3FE
UT WOS:000361215200001
ER
PT J
AU Hoffmann, R
Ferguson, D
Patton, J
Wheelock, AT
Young, JA
Crofton, MW
Prebola, JL
Crider, DH
Likar, JJ
Schneider, TA
Vaughn, JA
Bodeau, JM
Noushkam, N
Vayner, BV
Hoang, B
AF Hoffmann, Ryan
Ferguson, Dale
Patton, James
Wheelock, Adrian T.
Young, Jason A.
Crofton, Mark W.
Prebola, John L.
Crider, Dustin H.
Likar, Justin J.
Schneider, Todd A.
Vaughn, Jason A.
Bodeau, J. Michale
Noushkam, Nikki
Vayner, Boris V.
Hoang, Bao
TI AFRL Round-Robin Test Results on Plasma Propagation Velocity
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article; Proceedings Paper
CT 13th Spacecraft Charging Technology Conference
CY JUN 23-27, 2014
CL Pasadena, CA
DE Dielectric; discharge; flashover; spacecraft charging
ID SOLAR-ARRAY; FLASHOVER; EXPANSION
AB The speed plasma propagates across a charged solar panel after a primary arc is one of the most important, yet poorly known, quantities in determining Electrostatic Discharge (ESD) currents for spacecraft arcing events. A review of the literature over the last two decades reveals that measured propagation velocity varies by as much as an order of magnitude. To overcome this deficiency, a round-robin set of tests was initiated with partners from industry, academia, NASA and the U.S. Air Force. This paper will provide the most recent results from the Air Force Research Laboratory testing conducted at the Spacecraft Charging and Instrument Calibration Laboratory.
C1 [Hoffmann, Ryan; Ferguson, Dale; Patton, James; Wheelock, Adrian T.] Air Force Res Lab, Spacecraft Charging & Instrument Calibrat Lab, Kirtland AFB, NM 87117 USA.
[Young, Jason A.; Crofton, Mark W.] Aerosp Corp, Los Angeles, CA 90009 USA.
[Prebola, John L.; Crider, Dustin H.] Aerosp Testing Alliance, Arnold Afb, TN 37389 USA.
[Likar, Justin J.] UTC Aerosp Syst, Charlotte, NC 28217 USA.
[Schneider, Todd A.; Vaughn, Jason A.] NASA, Marshal Space Flight Ctr, Huntsville, AL 35812 USA.
[Bodeau, J. Michale] Northrop Grumman, Mclean, VA 22102 USA.
[Noushkam, Nikki] Orbital Sci, Chandler, AZ 85248 USA.
[Vayner, Boris V.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Hoang, Bao] Space Syst Loral, Palo Alto, CA 94303 USA.
RP Hoffmann, R (reprint author), Air Force Res Lab, Spacecraft Charging & Instrument Calibrat Lab, Kirtland AFB, NM 87117 USA.
EM ryan.hoffmann@us.af.mil; dale.ferguson@us.af.mil; james.patton@us.af.mil
FU Air Force Research Laboratory
FX This work was supported by the Air Force Research Laboratory.
(Corresponding author: Ryan Hoffmann.)
NR 21
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 0093-3813
EI 1939-9375
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD SEP
PY 2015
VL 43
IS 9
SI SI
BP 3006
EP 3013
DI 10.1109/TPS.2015.2465865
PN 1
PG 8
WC Physics, Fluids & Plasmas
SC Physics
GA CR3FE
UT WOS:000361215200031
ER
PT J
AU Ferguson, DC
Katz, I
AF Ferguson, Dale C.
Katz, Ira
TI The Worst Case GEO Environment and the Frequency of Arcs in GEO
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article; Proceedings Paper
CT 13th Spacecraft Charging Technology Conference
CY JUN 23-27, 2014
CL Pasadena, CA
DE GEO; plasmas; spacecraft charging; worst cases
AB Proper spacecraft design and testing depend on a knowledge of the worst case environment and the number of arcs to be endured during the spacecraft lifetime. In this paper, we define the criteria to be used to specify the worst case geosynchronous earth orbit (GEO) charging environment (plasma density and temperature), including the physical constraints on particle and magnetic field energy densities and the relative importance of frame charging and differential charging. A previous estimate of the frequency of arcing (found in the literature and incorporated into an International Standards Organization standard) and the consequent total number of arcs to be encountered in a GEO satellite lifetime are found to be incorrect because they were based on environmental measurements using a faulty algorithm to determine spacecraft charging and plasma density. Using more accurate estimates of the frequency of GEO plasma densities and temperatures, we arrive at a much lower estimate of the total number of arcs during a GEO satellite lifetime. Finally, the worst case GEO charging environment seen to date is determined from Nascap-2k simulations. Our estimates of worst case charging environments and arc frequencies may be more confidently used by GEO spacecraft designers and test engineers.
C1 [Ferguson, Dale C.] Air Force Res Lab, Albuquerque, NM 87117 USA.
[Katz, Ira] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ferguson, DC (reprint author), Air Force Res Lab, Albuquerque, NM 87117 USA.
EM dale.ferguson@kirtland.af.mil; ira.katz@jpl.nasa.gov
NR 17
TC 1
Z9 1
U1 1
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
EI 1939-9375
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD SEP
PY 2015
VL 43
IS 9
SI SI
BP 3021
EP 3026
DI 10.1109/TPS.2015.2432718
PN 1
PG 6
WC Physics, Fluids & Plasmas
SC Physics
GA CR3FE
UT WOS:000361215200033
ER
PT J
AU Capece, AM
Polk, JE
Shepherd, JE
AF Capece, Angela M.
Polk, James E.
Shepherd, Joseph E.
TI Decoupling the Thermal and Plasma Effects on the Operation of a Xenon
Hollow Cathode With Oxygen Poisoning Gas
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Barium; cathodes; electron emission; oxygen; poisoning
ID IMPREGNATED-CATHODE; MECHANISM; MODEL
AB Hollow cathodes are used as the electron source for generating the plasma discharge in electric thrusters. These cathodes contain porous tungsten emitters impregnated with BaO material to achieve a lower surface work function and are operated with xenon propellant. Reactive contaminants such as oxygen in the xenon gas can modify the surface chemistry and morphology of BaO dispenser cathodes and degrade the electron emission properties. Hollow cathodes that operate with reactive impurities in the propellant will experience higher operating temperatures, which increase the evaporation of the emission materials and reduce cathode life. A significant amount of work has been previously done to understand the effects of oxygen poisoning on vacuum cathodes; however, the xenon plasma adds complexity and its role during cathode poisoning is not completely understood. A deeper understanding of the mechanisms initiating cathode failure will improve the thruster operation, increase the lifetime, and ultimately reduce the cost. In this paper, we present the results of experiments in which the cathode was operated with 100 ppm of oxygen gas in the xenon plasma at two different discharge currents. Poisoning was indicated by an increase in the emitter temperature that was measured using a two-color pyrometer and thermocouples. The emitter temperature rose monotonically during poisoning and decayed to its original value when the oxygen flow was turned OFF, indicating that short exposures to oxygen do not result in permanent cathode damage. The experiments show that removal of oxygen adatoms from the cathode surface following poisoning is dominated by thermal desorption rather than xenon ion sputtering. Operation at higher discharge currents improves the resistance to poisoning as a result of the higher operating temperatures at these conditions.
C1 [Capece, Angela M.; Shepherd, Joseph E.] CALTECH, Pasadena, CA 91125 USA.
[Polk, James E.] Jet Prop Lab, Pasadena, CA 91109 USA.
RP Capece, AM (reprint author), Coll New Jersey, Ewing, NJ 08618 USA.
EM capecea@tcnj.edu; james.e.polk@jpl.nasa.gov;
joseph.e.shepherd@caltech.edu
RI Shepherd, Joseph/B-5997-2014
OI Shepherd, Joseph/0000-0003-3181-9310
FU Jet Propulsion Laboratory, Pasadena, CA, USA
FX This work was supported by the Jet Propulsion Laboratory, Pasadena, CA,
USA.
NR 22
TC 0
Z9 0
U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
EI 1939-9375
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD SEP
PY 2015
VL 43
IS 9
BP 3249
EP 3255
DI 10.1109/TPS.2015.2465845
PN 2
PG 7
WC Physics, Fluids & Plasmas
SC Physics
GA CR7KX
UT WOS:000361529600018
ER
PT J
AU Molod, A
Salmun, H
Dempsey, M
AF Molod, A.
Salmun, H.
Dempsey, M.
TI Estimating Planetary Boundary Layer Heights from NOAA Profiler Network
Wind Profiler Data
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID MIXING HEIGHT; DEPTH
AB An algorithm was developed to estimate planetary boundary layer (PBL) heights from hourly archived wind profiler data from the NOAA Profiler Network (NPN) sites located throughout the central United States. Unlike previous studies, the present algorithm has been applied to a long record of publicly available wind profiler signal backscatter data. Under clear-sky conditions, summertime averaged hourly time series of PBL heights compare well with Richardson number-based estimates at the few NPN stations with hourly temperature measurements. Comparisons with estimates based on clear-sky reanalysis show that the wind profiler (WP) PBL heights are lower by approximately 250-500 m. The geographical distribution of daily maximum PBL heights corresponds well with the expected distribution based on patterns of surface temperature and soil moisture. Wind profiler PBL heights were also estimated under mostly cloudy-sky conditions, and are generally comparable to the Richardson number-based PBL heights and higher than the reanalysis PBL heights. WP PBL heights have a smaller clear-cloudy condition difference than either of the other two. The algorithm presented here is shown to provide a reliable summertime climatology of daytime hourly PBL heights throughout the central United States.
C1 [Molod, A.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Salmun, H.] CUNY Hunter Coll, New York, NY 10021 USA.
[Salmun, H.; Dempsey, M.] CUNY, Grad Ctr, Earth & Environm Sci, New York, NY USA.
[Molod, A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Molod, A (reprint author), NASA Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM andrea.molod@nasa.gov
NR 26
TC 2
Z9 2
U1 1
U2 8
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 SEP
PY 2015
VL 32
IS 9
BP 1545
EP 1561
DI 10.1175/JTECH-D-14-00155.1
PG 17
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA CR5EY
UT WOS:000361364500001
ER
PT J
AU Lolli, S
Di Girolamo, P
AF Lolli, Simone
Di Girolamo, Paolo
TI Principal Component Analysis Approach to Evaluate Instrument
Performances in Developing a Cost-Effective Reliable Instrument Network
for Atmospheric Measurements
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID LIDAR
AB Developing a reliable cost-effective instrument network for data measurement is a challenging task for agency decisionmakers. A simple way to fully characterize the performances of an instrument that also considers economical and operational factors-price, maintenance cost, lifetime, etc.-currently does not exist. Through principal component analysis, a method is developed to build a composite index that assigns a single score to each instrument, taking into account all the scientific, economic, and operational aspects. This index will then represent solid help in building and optimizing a cost-effective network, bridging the gap between two very different worlds: the scientific need for precision and economic constraints.
C1 [Lolli, Simone] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Lolli, Simone] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Di Girolamo, Paolo] Univ Basilicata, Scuola Ingn, I-85100 Potenza, Italy.
RP Lolli, S (reprint author), NASA Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM simone.lolli@nasa.gov
NR 21
TC 2
Z9 2
U1 0
U2 0
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 SEP
PY 2015
VL 32
IS 9
BP 1642
EP 1649
DI 10.1175/JTECH-D-15-0085.1
PG 8
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA CR5EY
UT WOS:000361364500007
ER
PT J
AU Roth, DJ
Cosgriff, LM
Harder, B
Zhu, DM
Martins, RE
AF Roth, Don J.
Cosgriff, Laura M.
Harder, Bryan
Zhu, Dongming
Martins, Richard E.
TI Self-calibrating Terahertz Technique for Measuring Coating Thickness
SO MATERIALS EVALUATION
LA English
DT Article
DE terahertz; velocity; thickness; coatings; self-calibrating
ID THERMAL-BARRIER COATINGS
AB This study investigates the applicability of a novel noncontact single-sided terahertz electromagnetic measurement technique for measuring thickness in dielectric coating systems on simulated and real-world coating/substrate systems. The technique does not require knowledge of the velocity of terahertz waves in the coating material. The dielectric coatings ranged from approximately 200 to 1400 pm in thickness. The simulated coating consisted of layered thin paper samples of varying thicknesses on a superalloy substrate and the real-world system consisted of an actual thermal barrier coating on the superalloy substrate. The unique aspects and limitations of this technique for thickness measurements are discussed.
C1 [Roth, Don J.] NASA Glenn Res Ctr, ASNT NDT Level 3, Cleveland, OH 44135 USA.
[Harder, Bryan; Zhu, Dongming] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Martins, Richard E.] Cleveland State Univ, Cleveland, OH 44115 USA.
RP Roth, DJ (reprint author), NASA Glenn Res Ctr, ASNT NDT Level 3, Cleveland, OH 44135 USA.
NR 19
TC 0
Z9 0
U1 1
U2 2
PU AMER SOC NONDESTRUCTIVE TEST
PI COLUMBUS
PA 1711 ARLINGATE LANE PO BOX 28518, COLUMBUS, OH 43228-0518 USA
SN 0025-5327
J9 MATER EVAL
JI Mater. Eval.
PD SEP
PY 2015
VL 73
IS 9
BP 1205
EP 1213
PG 9
WC Materials Science, Characterization & Testing
SC Materials Science
GA CR4AD
UT WOS:000361273300030
ER
PT J
AU Luvall, JC
AF Luvall, J. C.
TI A new age in epidemiology - a thermodynamic paradigm for studying
disease vector's habitats and life cycles using NASA's remote sensing
data
SO TROPICAL MEDICINE & INTERNATIONAL HEALTH
LA English
DT Meeting Abstract
C1 [Luvall, J. C.] Nation Marshal Space Flight Ctr, Marshal Space Flight Ctr, Natl Space Sci & Technol Ctr, NASA, Huntsville, AL USA.
NR 0
TC 0
Z9 0
U1 2
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1360-2276
EI 1365-3156
J9 TROP MED INT HEALTH
JI Trop. Med. Int. Health
PD SEP
PY 2015
VL 20
SU 1
SI SI
MA PS2.293
BP 413
EP 413
PG 1
WC Public, Environmental & Occupational Health; Tropical Medicine
SC Public, Environmental & Occupational Health; Tropical Medicine
GA CQ7BW
UT WOS:000360758802272
ER
PT J
AU Sultana, J
Kazanas, D
AF Sultana, J.
Kazanas, D.
TI Inertia in Friedmann Universes with variable G and Lambda
SO ASTROPHYSICS AND SPACE SCIENCE
LA English
DT Article
DE Inertia; Friedmann Universes; Mach's Principle
ID COSMOLOGICAL MODELS; GRAVITATIONAL CONSTANT; MACHS PRINCIPLE;
DARK-MATTER; TERM; ORIGIN; HYPOTHESIS; GRAVITY; ENERGY; FIELDS
AB In light of the recent interest in dynamical dark energy models based on a cosmology with varying gravitational and cosmological parameters G and Lambda, we present here a model of inertia in a type of Friedmann universe with G=G(0)(A/A(0))(sigma); A being the dimensionless scale factor, that was recently studied by Singh et al. (Astrophys. Space Sci. 345: 213, 2013). The proposed Machian model of inertia utilizes the curved space generalization of Sciama's law of inertial induction, which is based on the analogy between the retarded far fields of electrodynamics and those of gravitation, and expresses the total inertial force F=-ma on an accelerating mass m in terms of contributions from all matter in the observable Universe. We show that for a varying Friedmann model with sigma=-3/2, inertial induction alone can account for the total inertial force on the accelerating mass. We then compare this cosmological model with current observational constraints for the variation of G.
C1 [Sultana, J.] Univ Malta, Fac Sci, Dept Math, Msida MSD2080, Malta.
[Kazanas, D.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Sultana, J (reprint author), Univ Malta, Fac Sci, Dept Math, Msida MSD2080, Malta.
EM joseph.sultana@um.edu.mt
FU University of Malta
FX J.S. gratefully acknowledges financial support from the University of
Malta during his visit at NASA-GSFC and the hospitality of the
Astrophysics Science Division of GSFC.
NR 68
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0004-640X
EI 1572-946X
J9 ASTROPHYS SPACE SCI
JI Astrophys. Space Sci.
PD SEP
PY 2015
VL 359
IS 1
AR 9
DI 10.1007/s10509-015-2452-y
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8EY
UT WOS:000360840500009
ER
PT J
AU Li, FL
Jo, YH
Yan, XH
Liu, WT
AF Li, Feili
Jo, Young-Heon
Yan, Xiao-Hai
Liu, W. Timothy
TI Varying temperature and heat content signatures in the central Labrador
Sea at different layers and timescales
SO DEEP-SEA RESEARCH PART I-OCEANOGRAPHIC RESEARCH PAPERS
LA English
DT Article
DE Deep ocean convection; Interannual thermal variability; Hilbert-Huang
transform; Global warming hiatus
ID SUBPOLAR NORTH-ATLANTIC; MERIDIONAL OVERTURNING CIRCULATION; EMPIRICAL
MODE DECOMPOSITION; THERMOHALINE CIRCULATION; DEEP CONVECTION; WATER
FORMATION; OCEAN; OSCILLATION; SALINITY; GYRE
AB The dominant modes of variability in the temperature and ocean heat content (OHC; 0-1000 m) of the central Labrador Sea were investigated using the Hilbert-Huang Transform (HHT) based on Argo profiles collected during 2003-2012. Warming trends of approximately 0.03 degrees C yr(-1) were observed in the upper 2000 m of the water column. A strong annual temperature cycle exists and dominates at the 500 m depth, while signals at the interannual timescales can explain most of the temperature variability at the 1000 m and 1500 m depths. These interannual signals are closely correlated to the variability of deep convection in the Labrador Sea, which has intermittent enhancement of mixed layer depth (MLD) > 1500 m. The Hilbert spectrum from the OHC in the Labrador Sea interior reveals two important components at frequencies of 0.8-1.2 cycle yr(-1) (T=0.8-1.25 years) and 0.1-0.3 cycle yr(-1) (T=3.3-10 years), respectively, superimposed on the warming trends. The former corresponds to the dominant seasonal cycle due to surface heating, while the latter is concomitant with the timing of the reoccurrence of convective events. We also found that the cumulative North Atlantic Oscillation (NAO) index significantly correlates to the low-frequency OHC variations. Therefore, the interannual signals in the Labrador Sea at especially the intermediate layers are attributed to changes in the deep convective processes and the atmospheric conditions. By comparing with an extended OHC record (1945-2010), it was further shown that the warming trends obtained from the 10-year Argo record are part of multi-decadal variations that presumably reflect the Atlantic Multi-decadal Oscillation (AMC). In addition, the recent OHC changes in the Labrador Sea (i.e., increased heat in the deeper layers) may be related to the current global warming hiatus, suggesting the potential contributions from the Atlantic Meridional Overturning Circulation (AMOC) to the low-frequency OHC in the Labrador Sea. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Li, Feili; Jo, Young-Heon; Yan, Xiao-Hai] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA.
[Yan, Xiao-Hai] Univ Delaware, Xiamen Univ, Joint Inst Coastal Res & Management, Newark, DE 19716 USA.
[Liu, W. Timothy] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Yan, XH (reprint author), Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA.
EM xiaohai@udel.edu
FU NASA Physical Oceanography Program; NASA EPSCoR Program; NASA Space
Grant; NOAA Sea Grant
FX The authors thank three anonymous reviewers for their helpful comments
that greatly improved this manuscript. The Argo data was collected from
the Global Argo Data Repository (GADR) operated by the U.S. National
Oceanographic Data Center (NODC). The Climate Data Guide: Hurrell North
Atlantic Oscillation (NAO) Index (station-based) was provided by
Hurrell, James & National Center for Atmospheric Research Staff (Eds).
Ocean heat content (OHC) analysis is based on Ishii and Kimoto (2009).
This research was partially supported by NASA Physical Oceanography
Program, NASA EPSCoR Program, NASA Space Grant, and NOAA Sea Grant. The
authors thank Federico lenna for proof reading the article.
NR 70
TC 0
Z9 0
U1 2
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0637
EI 1879-0119
J9 DEEP-SEA RES PT I
JI Deep-Sea Res. Part I-Oceanogr. Res. Pap.
PD SEP
PY 2015
VL 103
BP 114
EP 124
DI 10.1016/j.dsr.2015.04.012
PG 11
WC Oceanography
SC Oceanography
GA CQ8PU
UT WOS:000360871700010
ER
PT J
AU Lever, MA
Rogers, KL
Lloyd, KG
Overmann, J
Schink, B
Thauer, RK
Hoehler, TM
Jorgensen, BB
AF Lever, Mark A.
Rogers, Karyn L.
Lloyd, Karen G.
Overmann, Joerg
Schink, Bernhard
Thauer, Rudolf K.
Hoehler, Tori M.
Jorgensen, Bo Barker
TI Life under extreme energy limitation: a synthesis of laboratory- and
field-based investigations
SO FEMS MICROBIOLOGY REVIEWS
LA English
DT Review
DE energy limitation; microbial life; laboratory; starvation; subseafloor;
adaptation
ID MARINE VIBRIO SP; SULFATE-REDUCING BACTERIA; LONG-TERM STARVATION; DEEP
SUBSEAFLOOR SEDIMENTS; DISSOLVED ORGANIC-MATTER; MESSENGER-RNA
STABILITY; SINGLE-CELL ANALYSIS; FATTY-ACID PROFILES; SP STRAIN S14;
ESCHERICHIA-COLI
AB The ability of microorganisms to withstand long periods with extremely low energy input has gained increasing scientific attention in recent years. Starvation experiments in the laboratory have shown that a phylogenetically wide range of microorganisms evolve fitness-enhancing genetic traits within weeks of incubation under low-energy stress. Studies on natural environments that are cut off from new energy supplies over geologic time scales, such as deeply buried sediments, suggest that similar adaptations might mediate survival under energy limitation in the environment. Yet, the extent to which laboratory-based evidence of starvation survival in pure or mixed cultures can be extrapolated to sustained microbial ecosystems in nature remains unclear. In this review, we discuss past investigations on microbial energy requirements and adaptations to energy limitation, identify gaps in our current knowledge, and outline possible future foci of research on life under extreme energy limitation.This is a synthesis of laboratory- and field-based investigations on microbial life under energy limitation.This is a synthesis of laboratory- and field-based investigations on microbial life under energy limitation.
C1 [Lever, Mark A.; Jorgensen, Bo Barker] Aarhus Univ, Inst Biosci, Ctr Geomicrobiol, DK-8000 Aarhus C, Denmark.
[Rogers, Karyn L.] Rensselaer Polytech Inst, Earth & Environm Sci, Jonsson Rowland Sci Ctr, Troy, NY 12180 USA.
[Lloyd, Karen G.] Univ Tennessee, Dept Microbiol, Knoxville, TN 37996 USA.
[Overmann, Joerg] Deutsch Sammlung von Mikroorganismen & Zellkultur, Leibniz Inst DSMZ, D-38124 Braunschweig, Germany.
[Schink, Bernhard] Univ Konstanz, Dept Biol, Microbial Ecol, D-78457 Constance, Germany.
[Thauer, Rudolf K.] Max Planck Inst Terr Mikrobiol, D-35043 Marburg, Germany.
[Hoehler, Tori M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lever, MA (reprint author), ETH, Dept Environm Syst Sci, Inst Biogeochem & Pollutant Dynam, Univ Str 16, CH-8092 Zurich, Switzerland.
EM mark.lever@usys.ethz.ch
RI Rogers, Karyn/K-7670-2015; Jorgensen, Bo/C-2214-2013; Lever, Mark
Alexander/C-2134-2011
OI Jorgensen, Bo/0000-0001-9398-8027; Lever, Mark
Alexander/0000-0002-2046-8028
FU Marie-Curie Intra-European Fellowship [255135]; NASA [NNX08AY55A];
Center for Dark Energy Biosphere Investigations (C-DEBI) [42525882,
OCE-0939564]; ERC under the EU; Danish National Research Foundation; Max
Planck Society
FX Personal financial support was obtained from a Marie-Curie
Intra-European Fellowship to M. Lever (#255135), a grant from the NASA
Exobiology program (NNX08AY55A) to K. Rogers, a grant from the Center
for Dark Energy Biosphere Investigations (C-DEBI) (Award# 42525882,
Prime Award# OCE-0939564) to K. Lloyd, and the ERC Advanced Grant
'Microbial life under extreme energy limitation (MICROENERGY)' to B. B.
Jorgensen under the EU 7th FP. Funding support for the workshop was to
B. B. Jorgensen and was obtained from the Danish National Research
Foundation and the Max Planck Society. This is C-DEBI publication 260.
NR 350
TC 28
Z9 28
U1 14
U2 62
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0168-6445
EI 1574-6976
J9 FEMS MICROBIOL REV
JI Fems Microbiol. Rev.
PD SEP
PY 2015
VL 39
IS 5
BP 688
EP 728
DI 10.1093/femsre/fuv020
PG 41
WC Microbiology
SC Microbiology
GA CR3CY
UT WOS:000361209300004
PM 25994609
ER
PT J
AU Lee, JE
Berry, JA
Van der Tol, CS
Yang, X
Guanter, L
Damm, A
Baker, I
Frankenberg, C
AF Lee, Jung-Eun
Berry, Joseph A.
Van der Tol, Chri Stiaan
Yang, Xi
Guanter, Luis
Damm, Alexander
Baker, Ian
Frankenberg, Christian
TI Simulations of chlorophyll fluorescence incorporated into the Community
Land Model version 4
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE chlorophyll fluorescence; GOSAT; gross primary production; land surface
model; model evaluation; NCAR CLM; remote sensing; tropical forests
ID SUN-INDUCED FLUORESCENCE; STOMATAL CONDUCTANCE; SOIL-MOISTURE;
WATER-STRESS; LEAF; PHOTOSYNTHESIS; PLANTS; CLIMATE; CANOPY; REFLECTANCE
AB Several studies have shown that satellite retrievals of solar-induced chlorophyll fluorescence (SIF) provide useful information on terrestrial photosynthesis or gross primary production (GPP). Here, we have incorporated equations coupling SIF to photosynthesis in a land surface model, the National Center for Atmospheric Research Community Land Model version 4 (NCAR CLM4), and have demonstrated its use as a diagnostic tool for evaluating the calculation of photosynthesis, a key process in a land surface model that strongly influences the carbon, water, and energy cycles. By comparing forward simulations of SIF, essentially as a byproduct of photosynthesis, in CLM4 with observations of actual SIF, it is possible to check whether the model is accurately representing photosynthesis and the processes coupled to it. We provide some background on how SIF is coupled to photosynthesis, describe how SIF was incorporated into CLM4, and demonstrate that our simulated relationship between SIF and GPP values are reasonable when compared with satellite (Greenhouse gases Observing SATellite; GOSAT) and in situ flux-tower measurements. CLM4 overestimates SIF in tropical forests, and we show that this error can be corrected by adjusting the maximum carboxylation rate (V-max) specified for tropical forests in CLM4. Our study confirms that SIF has the potential to improve photosynthesis simulation and thereby can play a critical role in improving land surface and carbon cycle models.
C1 [Lee, Jung-Eun; Yang, Xi] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
[Berry, Joseph A.; Van der Tol, Chri Stiaan] Univ Twente, Geoinformat Sci & Earth Observat, NL-7500 AE Enschede, Netherlands.
[Berry, Joseph A.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[Guanter, Luis] GFZ German Res Ctr Geosci, Helmholtz Ctr Potsdam, D-14473 Potsdam, Germany.
[Damm, Alexander] Univ Zurich, Dept Geog, Remote Sensing Labs, CH-8057 Zurich, Switzerland.
[Baker, Ian] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lee, JE (reprint author), Brown Univ, Dept Earth Environm & Planetary Sci, POB 1846 324,Brook St, Providence, RI 02912 USA.
EM leeje@brown.edu
RI van der Tol, Christiaan/A-2403-2010; Frankenberg, Christian/A-2944-2013;
OI van der Tol, Christiaan/0000-0002-2484-8191; Frankenberg,
Christian/0000-0002-0546-5857; Yang, Xi/0000-0002-5095-6735
FU DOE GOAmazon Program [DE-FG02-14ER65585]; Brown University
FX JEL thanks T. Webb, A. Kornfeld, E. Robinson, A. Chang, and anonymous
reviewers for helpful comments on the earlier version of the paper. The
authors thank R. Hutjes for making the flux-tower data available. The
authors also benefitted from discussion during a workshop arranged by
the W.M. Keck Institute for Space Studies. This work was supported by
DOE GOAmazon Program (DE-FG02-14ER65585) and Brown University. The model
simulations were performed on Yellowstone, and JEL thanks G. Bonan for
the support.
NR 45
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Z9 8
U1 12
U2 58
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
EI 1365-2486
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD SEP
PY 2015
VL 21
IS 9
BP 3469
EP 3477
DI 10.1111/gcb.12948
PG 9
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA CR0HE
UT WOS:000360998400025
PM 25881891
ER
PT J
AU Muller, CL
Chapman, L
Johnston, S
Kidd, C
Illingworth, S
Foody, G
Overeem, A
Leigh, RR
AF Muller, C. L.
Chapman, L.
Johnston, S.
Kidd, C.
Illingworth, S.
Foody, G.
Overeem, A.
Leigh, R. R.
TI Crowdsourcing for climate and atmospheric sciences: current status and
future potential
SO INTERNATIONAL JOURNAL OF CLIMATOLOGY
LA English
DT Review
DE Internet of things; Big data; Citizen science; Sensors; Amateur;
Applications
ID VOLUNTEERED GEOGRAPHIC INFORMATION; URBAN METEOROLOGICAL NETWORKS;
CITIZEN-SCIENCE; RAIN GAUGES; COMMUNICATION-NETWORKS; PRESSURE
OBSERVATIONS; MOVING CARS; HEAT-ISLAND; QUALITY; TEMPERATURE
AB Crowdsourcing is traditionally defined as obtaining data or information by enlisting the services of a (potentially large) number of people. However, due to recent innovations, this definition can now be expanded to include and/or from a range of public sensors, typically connected via the Internet.' A large and increasing amount of data is now being obtained from a huge variety of non-traditional sources-from smart phone sensors to amateur weather stations to canvassing members of the public. Some disciplines (e.g. astrophysics, ecology) are already utilizing crowdsourcing techniques (e.g. citizen science initiatives, web 2.0 technology, low-cost sensors), and while its value within the climate and atmospheric science disciplines is still relatively unexplored, it is beginning to show promise. However, important questions remain; this paper introduces and explores the wide-range of current and prospective methods to crowdsource atmospheric data, investigates the quality of such data and examines its potential applications in the context of weather, climate and society. It is clear that crowdsourcing is already a valuable tool for engaging the public, and if appropriate validation and quality control procedures are adopted and implemented, it has much potential to provide a valuable source of high temporal and spatial resolution, real-time data, especially in regions where few observations currently exist, thereby adding value to science, technology and society.
C1 [Muller, C. L.; Chapman, L.] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England.
[Johnston, S.] OpenSignal, London, England.
[Kidd, C.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, Baltimore, MD USA.
[Kidd, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Illingworth, S.] Manchester Metropolitan Univ, Sch Res Enterprise & Innovat, Manchester M15 6BH, Lancs, England.
[Foody, G.] Univ Nottingham, Sch Geog, Nottingham NG7 2RD, England.
[Overeem, A.] Wageningen Univ, Hydrol & Quantitat Water Management Grp, NL-6700 AP Wageningen, Netherlands.
[Overeem, A.] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands.
[Leigh, R. R.] Univ Leicester, Earth Observat Sci Phys & Astron, Leicester LE1 7RH, Leics, England.
RP Muller, CL (reprint author), Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England.
EM c.l.muller@bham.ac.uk
RI Chapman, Lee/F-4674-2014; Illingworth, Samuel/A-4899-2015;
OI Chapman, Lee/0000-0002-2837-8334; Illingworth,
Samuel/0000-0003-2551-0675; Overeem, Aart/0000-0001-5550-8141
FU UK Natural Environmental Research Council (NERC) [NE/I006915/1,
NE/I029293/1]; Netherlands Technology Foundation STW [11944]; UK NERC
National Centre for Earth Observation (NCEO); Open Knowledge Foundation
Panton Fellowship
FX The authors would like to thank the UK Natural Environmental Research
Council (NERC) for funding Dr Catherine Muller (NE/I006915/1), Dr Lee
Chapman (NE/I006915/1), and Dr Illingworth (NE/I029293/1); The
Netherlands Technology Foundation STW for supporting Dr Aart Overeem
(project 11944); The UK NERC National Centre for Earth Observation
(NCEO) for supporting Dr Rosemarie Graves, who also holds an Open
Knowledge Foundation Panton Fellowship; Samuel Johnston would like to
acknowledge James Robinson, CTO OpenSignal. The Authors would also like
to thank Dr Andrew Hudson-Smith at the Centre for Advanced Spatial
Analysis, University College London, Dr Geoff Jenkins from the UK Met
Office Hadley Centre for Climate Prediction and Research, and the
anonymous reviewers for their comments and insights while preparing this
manuscript.
NR 135
TC 16
Z9 17
U1 12
U2 72
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0899-8418
EI 1097-0088
J9 INT J CLIMATOL
JI Int. J. Climatol.
PD SEP
PY 2015
VL 35
IS 11
BP 3185
EP 3203
DI 10.1002/joc.4210
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CQ9FF
UT WOS:000360917500001
ER
PT J
AU Seager, R
Hoerling, M
Schubert, S
Wang, HL
Lyon, B
Kumar, A
Nakamura, J
Henderson, N
AF Seager, Richard
Hoerling, Martin
Schubert, Siegfried
Wang, Hailan
Lyon, Bradfield
Kumar, Arun
Nakamura, Jennifer
Henderson, Naomi
TI Causes of the 2011-14 California Drought*
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; SOUTHWESTERN NORTH-AMERICA; UNITED-STATES;
PACIFIC-OCEAN; EL-NINO; ATMOSPHERIC VARIABILITY; GROUNDWATER DEPLETION;
SOUTHERN OSCILLATION; GREAT-PLAINS; LA-NINA
AB The causes of the California drought during November-April winters of 2011/12-2013/14 are analyzed using observations and ensemble simulations with seven atmosphere models forced by observed SSTs. Historically, dry California winters are most commonly associated with a ridge off the west coast but no obvious SST forcing. Wet winters are most commonly associated with a trough off the west coast and an El Nino event. These attributes of dry and wet winters are captured by many of the seven models. According to the models, SST forcing can explain up to a third of California winter precipitation variance. SST forcing was key to sustaining a high pressure ridge over the west coast and suppressing precipitation during the three winters. In 2011/12 this was a response to a La Nina event, whereas in 2012/13 and 2013/14 it appears related to a warm west-cool east tropical Pacific SST pattern. All models contain a mode of variability linking such tropical Pacific SST anomalies to a wave train with a ridge off the North American west coast. This mode explains less variance than ENSO and Pacific decadal variability, and its importance in 2012/13 and 2013/14 was unusual. The models from phase 5 of CMIP (CMIP5) project rising greenhouse gases to cause changes in California all-winter precipitation that are very small compared to recent drought anomalies. However, a long-term warming trend likely contributed to surface moisture deficits during the drought. As such, the precipitation deficit during the drought was dominated by natural variability, a conclusion framed by discussion of differences between observed and modeled tropical SST trends.
C1 [Seager, Richard; Nakamura, Jennifer; Henderson, Naomi] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Hoerling, Martin] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Schubert, Siegfried; Wang, Hailan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lyon, Bradfield] Columbia Univ, Int Res Inst Climate & Soc, Palisades, NY 10964 USA.
[Kumar, Arun] NOAA, Climate Predict Ctr, College Pk, MD USA.
RP Seager, R (reprint author), Columbia Univ, Lamont Doherty Earth Observ, 61 Route 9W, Palisades, NY 10964 USA.
EM seager@ldeo.columbia.edu
FU NSF [AGS-1401400, AGS-1243204]; NOAA [NA10OAR4310137, NA14OAR4310232]
FX This work was initiated by the NOAA Drought Task Force, and we thank
Annarita Mariotti and Dan Barrie for organizational efforts and
encouragement. We also thank Tom Delworth, Dan Cayan, Kelly Redmond, and
an anonymous reviewer for their very valuable comments and criticisms on
the NOAA report that was the basis for this paper. R.S., N.H., and J.N.
were supported by NSF Awards AGS-1401400 and AGS-1243204 and NOAA Awards
NA10OAR4310137(Global Decadal Hydroclimate Variability and Change) and
NA14OAR4310232. We thank Haibo Liu for assembling at LDEO the CMIP5 data
for analysis. We thank two reviewers plus Tony Broccoli for their
excellent and insightful reviews of the manuscript.
NR 75
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Z9 36
U1 26
U2 127
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD SEP
PY 2015
VL 28
IS 18
BP 6997
EP 7024
DI 10.1175/JCLI-D-14-00860.1
PG 28
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CR0TT
UT WOS:000361036800001
ER
PT J
AU D'Adderio, LP
Porcu, F
Tokay, A
AF D'Adderio, Leo Pio
Porcu, Federico
Tokay, Ali
TI Identification and Analysis of Collisional Breakup in Natural Rain
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID FRAGMENT SIZE DISTRIBUTIONS; COALESCENCE EFFICIENCIES; OPTICAL
DISDROMETER; DOPPLER RADAR; WATER DROPS; RAINDROPS; VELOCITY; SPECTRA;
SHAPES; PARAMETERIZATIONS
AB Numerous laboratory and numerical studies have been dedicated to understanding collisional breakup as one of the most important processes in rain formation. The present study aims to identify when, in natural rain, collisional breakup is dominant and thus able to modify the shape of the raindrop size distribution (DSD), up to the equilibrium DSD. To this end, an automated objective algorithm has been developed and applied to a total of more than 6000 two-minute-averaged DSDs. Since breakup is mostly observed in heavy precipitation, the method was applied to the DSDs where rain rate was above 5 mm h(-1). The selected breakup DSDs had good agreement with those predicted to be the equilibrium DSD by different theoretical models. The equilibrium DSD was found in a variable fraction of the total samples (0%-7%), confirming that the onset of equilibrium is a rare event in natural rain. The occurrence of a DSD in which breakup is dominant and modifies the DSD but the equilibrium DSD is not reached is higher (15%-47%). The gamma distribution, which has been widely used in the parameterization of observed size spectra, had a poor fitting in breakup-induced DSD, especially in the 1.0-2.6-mm-diameter interval. This can impact applications for which the parameterization of DSD is needed, such as in the retrieval of a DSD integral parameter (such as rain rate) from active remote sensor data.
C1 [D'Adderio, Leo Pio] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy.
[Porcu, Federico] Univ Bologna, Dept Phys & Astron, Bologna, Italy.
[Tokay, Ali] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP D'Adderio, LP (reprint author), Univ Ferrara, Dept Phys & Earth Sci, Via Saragat 1, I-44122 Ferrara, Italy.
EM dadderio@fe.infn.it
RI Measurement, Global/C-4698-2015;
OI Porcu, Federico/0000-0003-1283-7679
FU European Commission as part of the CEOP-AEGIS project [FP7-ENV-2007-1,
212921]
FX This study was partially funded by the European Commission (Call
FP7-ENV-2007-1 Grant 212921) as part of the CEOP-AEGIS project
coordinated by the Universite de Strasbourg, and by the "Bando per
soggiorno all'estero" of the University Institute for Higher Studies,
(IUSS-Ferrara 1391) of the University of Ferrara. Thanks to Patrick N.
Gatlin of the NASA Marshall Space Flight Center and Matthew Wingo of the
University of Alabama at Huntsville for maintenance of 2DVD during the
NASA Global Precipitation Measurement (GPM) mission ground validation
field campaigns led by Walter Petersen of the NASA Wallops Flight
Facility. We thank Robert Meneghini of the NASA Goddard Space Flight
Center and Xiaowen Li of Morgan State University for useful discussions.
The efforts of Ana Barros (Duke University) and two anonymous reviewers
contributed to increase the quality of this paper.
NR 57
TC 5
Z9 5
U1 2
U2 13
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 SEP
PY 2015
VL 72
IS 9
BP 3404
EP 3416
DI 10.1175/JAS-D-14-0304.1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CR0TW
UT WOS:000361037100008
ER
PT J
AU Moothi, K
Simate, GS
Falcon, R
Iyuke, SE
Meyyappan, M
AF Moothi, Kapil
Simate, Geoffrey S.
Falcon, Rosemary
Iyuke, Sunny E.
Meyyappan, M.
TI Carbon Nanotube Synthesis Using Coal Pyrolysis
SO LANGMUIR
LA English
DT Article
ID ENERGY MINIMIZATION APPROACH; ARC PLASMA CONDITIONS; SOLID FUELS;
GASIFICATION; KINETICS; MODEL; DEVOLATILISATION; PURIFICATION;
TEMPERATURE; CONVERSION
AB This study investigates carbon nanotube (CNT) production from coal pyrolysis wherein the output gases are used in a chemical vapor deposition reactor. The carbon products are similar to those using commercial coal gas as feedstock, but coal is relatively cheaper feedstock compared to high purity source gases. A Gibbs minimization model has, been developed to predict the volume percentages of product gases from coal pyrolysis. Methane and carbon monoxide were the largest carbon components of the product stream and thus formed the primary source for CNT synthesis. Both the model and the observations showed that increasing the furnace temperature led to a decrease in the absolute quantities of "useful" product gases, with the optimal temperature between 400 and 500 degrees C. Based on the experimental data, a kinetic rate law for CNT from coal pyrolysis was derived as d[CNT]/dt = K([CO][CH4])(1/2), where K is a function of several equilibrium constants representing various reactions in the CNT formation process.
C1 [Moothi, Kapil; Simate, Geoffrey S.; Falcon, Rosemary; Iyuke, Sunny E.] Univ Witwatersrand, Sch Chem & Met Engn, ZA-2050 Johannesburg, South Africa.
[Moothi, Kapil; Iyuke, Sunny E.] Univ Witwatersrand, DST NRF Ctr Excellence Strong Mat, ZA-2050 Johannesburg, South Africa.
[Meyyappan, M.] NASA Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
RP Iyuke, SE (reprint author), Univ Witwatersrand, Sch Chem & Met Engn, ZA-2050 Johannesburg, South Africa.
EM Sunny.Iyuke@wits.ac.za
OI Moothi, Kapil/0000-0001-7755-5125
FU National Research Foundation (NRF) under South Africa Focus Area, NRF
Nanotechnology flagship programme; Department of Science and Technology
(DST); DST/NRF Centre of Excellence
FX The authors acknowledge the financial support from the National Research
Foundation (NRF) under South Africa Focus Area, NRF Nanotechnology
flagship programme, Department of Science and Technology (DST)-funded
Chair of Clean Coal Technology grant, and DST/NRF Centre of Excellence.
The student bursaries provided by the University of the Witwatersrand
are acknowledged. Special thanks are due to S. Lekeletsan, D. Moor, and
L. Del for their help with laboratory testing.
NR 28
TC 2
Z9 2
U1 6
U2 31
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0743-7463
J9 LANGMUIR
JI Langmuir
PD SEP 1
PY 2015
VL 31
IS 34
BP 9464
EP 9472
DI 10.1021/acs.langmuir.5b01894
PG 9
WC Chemistry, Multidisciplinary; Chemistry, Physical; Materials Science,
Multidisciplinary
SC Chemistry; Materials Science
GA CQ7HG
UT WOS:000360773000023
PM 26262467
ER
PT J
AU Davies, LJM
Robotham, ASG
Driver, SP
Alpaslan, M
Baldry, IK
Bland-Hawthorn, J
Brough, S
Brown, MJI
Cluver, ME
Drinkwater, MJ
Foster, C
Grootes, MW
Konstantopoulos, IS
Lara-Lopez, MA
Lopez-Sanchez, AR
Loveday, J
Meyer, MJ
Moffett, AJ
Norberg, P
Owers, MS
Popescu, CC
De Propris, R
Sharp, R
Tuffs, RJ
Wang, L
Wilkins, SM
Dunne, L
Bourne, N
Smith, MWL
AF Davies, L. J. M.
Robotham, A. S. G.
Driver, S. P.
Alpaslan, M.
Baldry, I. K.
Bland-Hawthorn, J.
Brough, S.
Brown, M. J. I.
Cluver, M. E.
Drinkwater, M. J.
Foster, C.
Grootes, M. W.
Konstantopoulos, I. S.
Lara-Lopez, M. A.
Lopez-Sanchez, A. R.
Loveday, J.
Meyer, M. J.
Moffett, A. J.
Norberg, P.
Owers, M. S.
Popescu, C. C.
De Propris, R.
Sharp, R.
Tuffs, R. J.
Wang, L.
Wilkins, S. M.
Dunne, L.
Bourne, N.
Smith, M. W. L.
TI Galaxy And Mass Assembly (GAMA): the effect of close interactions on
star formation in galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: interactions; galaxies: star formation
ID DIGITAL SKY SURVEY; SUPERMASSIVE BLACK-HOLES; STELLAR MASS; FORMATION
RATES; REDSHIFT SURVEY; FORMATION HISTORIES; STARBURST GALAXIES;
LUMINOSITY DENSITY; FORMING GALAXIES; MERGING GALAXIES
AB The modification of star formation (SF) in galaxy interactions is a complex process, with SF observed to be both enhanced in major mergers and suppressed in minor pair interactions. Such changes likely to arise on short time-scales and be directly related to the galaxy-galaxy interaction time. Here we investigate the link between dynamical phase and direct measures of SF on different time-scales for pair galaxies, targeting numerous star-formation rate (SFR) indicators and comparing to pair separation, individual galaxy mass and pair mass ratio. We split our sample into the higher (primary) and lower (secondary) mass galaxies in each pair and find that SF is indeed enhanced in all primary galaxies but suppressed in secondaries of minor mergers. We find that changes in SF of primaries are consistent in both major and minor mergers, suggesting that SF in the more massive galaxy is agnostic to pair mass ratio. We also find that SF is enhanced/suppressed more strongly for short-duration SFR indicators (e.g. Ha), highlighting recent changes to SF in these galaxies, which are likely to be induced by the interaction. We propose a scenario where the lower mass galaxy has its SF suppressed by gas heating or stripping, while the higher mass galaxy has its SF enhanced, potentially by tidal gas turbulence and shocks. This is consistent with the seemingly contradictory observations for both SF suppression and enhancement in close pairs.
C1 [Davies, L. J. M.; Robotham, A. S. G.; Driver, S. P.; Meyer, M. J.; Moffett, A. J.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia.
[Driver, S. P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Alpaslan, M.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Baldry, I. K.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
[Bland-Hawthorn, J.] Univ Sydney, Sydney Inst Astron, Sch Phys A28, Sydney, NSW 2006, Australia.
[Brough, S.; Foster, C.; Konstantopoulos, I. S.; Lopez-Sanchez, A. R.; Owers, M. S.] Australian Astron Observ, N Ryde, NSW 1670, Australia.
[Brown, M. J. I.] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia.
[Cluver, M. E.] Univ Western Cape, ZA-7535 Cape Town, South Africa.
[Drinkwater, M. J.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia.
[Grootes, M. W.; Tuffs, R. J.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Lara-Lopez, M. A.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Lopez-Sanchez, A. R.; Owers, M. S.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Loveday, J.; Wilkins, S. M.] Univ Sussex, Dept Phys & Astron, Astron Ctr, Brighton BN1 9QH, E Sussex, England.
[Norberg, P.; Wang, L.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Popescu, C. C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Popescu, C. C.] Acad Romana, Astron Inst, Bucharest, Romania.
[De Propris, R.] Univ Turku, Finnish Ctr Astron ESO, FI-21500 Piikkio, Finland.
[Sharp, R.] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Wang, L.] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands.
[Dunne, L.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand.
[Dunne, L.; Bourne, N.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Smith, M. W. L.] Cardiff Univ, Sch Phys & Astron, Parade, Cardiff CF24 3AA, S Glam, Wales.
RP Davies, LJM (reprint author), Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia.
EM luke.j.davies@uwa.edu.au
RI Drinkwater, Michael/A-2201-2008; Brown, Michael/B-1181-2015;
OI Drinkwater, Michael/0000-0003-4867-0022; Brown,
Michael/0000-0002-1207-9137; Owers, Matt/0000-0002-2879-1663; Robotham,
Aaron/0000-0003-0429-3579; Alpaslan, Mehmet/0000-0003-0321-1033; Foster,
Caroline/0000-0003-0247-1204; Baldry, Ivan/0000-0003-0719-9385
FU STFC (UK); ARC (Australia); AAO; Australian Research Council
[FT100100280]; EC FP7 SPACE project ASTRODEEP [312725]; European
Research Council Advanced Investigator grant COSMICSM
FX GAMA is a joint European-Australasian project based around a
spectroscopic campaign using the Anglo-Australian Telescope. The GAMA
input catalogue is based on data taken from the Sloan Digital Sky Survey
and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the
GAMA regions is being obtained by a number of independent survey
programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE,
Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is
funded by the STFC (UK), the ARC (Australia), the AAO and the
participating institutions. The GAMA website is
http://www.gama-survey.org/. MJIB acknowledges financial support from
the Australian Research Council (FT100100280). NB acknowledges support
from the EC FP7 SPACE project ASTRODEEP (Ref. no. 312725). L. Dunne
acknowledges support from European Research Council Advanced
Investigator grant COSMICSM.
NR 75
TC 11
Z9 11
U1 1
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 SEP 1
PY 2015
VL 452
IS 1
BP 616
EP 636
DI 10.1093/mnras/stv1241
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8IP
UT WOS:000360851100046
ER
PT J
AU Sakurai, Y
Hosokawa, T
Yoshida, N
Yorke, HW
AF Sakurai, Y.
Hosokawa, T.
Yoshida, N.
Yorke, H. W.
TI Formation of primordial supermassive stars by burst accretion
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: formation; galaxies: formation; cosmology: theory; early Universe
ID MASSIVE BLACK-HOLES; ATOMIC COOLING HALOES; 1ST STARS; DIRECT COLLAPSE;
SUPERGIANT PROTOSTARS; EARLY UNIVERSE; EVOLUTION; FEEDBACK; SIMULATIONS;
REDSHIFT
AB Recent observations show that supermassive black holes (BHs) with similar to 10(9) M-circle dot exist at redshift z greater than or similar to 6. A promising formation channel is the so-called direct collapse model, which posits that a massive seed BH forms through gravitational collapse of a similar to 10(5) M-circle dot supermassive star (SMS). We study the evolution of such an SMS growing by rapid mass accretion. In particular, we examine the impact of time-dependent mass accretion of repeating burst and quiescent phases expected to occur with a self-gravitating circumstellar disc. We show that protostars growing via episodic accretion can substantially contract during the quiescent phases, in contrast to the case of constant mass accretion, whereby the star expands roughly monotonically. The stellar effective temperature and ionizing photon emissivity increase accordingly, which can cause strong ionizing feedback and halt the mass accretion. With a fixed duration of the quiescent phase Delta t(q), this contraction occurs in early evolutionary phases, i.e. for M-* less than or similar to 10(3) M-circle dot with Delta t(q) similar or equal to 10(3) yr. For later epochs and larger masses but the same Delta t(q), contraction is negligible even during quiescent phases. With larger Delta t(q), however, the star continues to contract during quiescent phases even for the higher stellar masses. We show that this behaviour is well understood by comparing the interval time and the thermal relaxation time for a bloated surface layer. We conclude that the feedback becomes effective, if Delta t(q) greater than or similar to 10(3) yr, which is possible in an accretion disc forming in the direct collapse model.
C1 [Sakurai, Y.] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan.
[Hosokawa, T.] Univ Tokyo, Dept Phys & Res Ctr Early Univ, Tokyo 1130033, Japan.
[Yoshida, N.] Univ Tokyo, Kavli Inst Phys & Math Univ WPI, Kashiwa, Chiba 2778583, Japan.
[Yorke, H. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sakurai, Y (reprint author), Univ Tokyo, Dept Phys, Tokyo 1130033, Japan.
EM sakurai@utap.phys.s.u-tokyo.ac.jp
FU Advanced Leading Graduate Course for Photon Science; JSPS Promotion of
Science [25800102, 15H00776, 25287050, 15J08816]; National Aeronautics
and Space Administration (NASA)
FX We thank Kazuyuki Omukai, Kohei Inayoshi and Eduard Vorobyov for
fruitful discussions. The calculations were in part carried out on PC
cluster at Center for Computational Astrophysics, National Astronomical
Observatory of Japan. YS is supported by Advanced Leading Graduate
Course for Photon Science. This work is supported in part by
Grant-in-Aid for Scientific Research from the JSPS Promotion of Science
(25800102, 15H00776, 25287050, and 15J08816). Portions of this research
were conducted at the Jet Propulsion Laboratory, California Institute of
Technology, operating under a contract with the National Aeronautics and
Space Administration (NASA).
NR 49
TC 13
Z9 13
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 SEP 1
PY 2015
VL 452
IS 1
BP 755
EP 764
DI 10.1093/mnras/stv1346
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8IP
UT WOS:000360851100055
ER
PT J
AU Kearney, SP
Danehy, PM
AF Kearney, Sean P.
Danehy, Paul M.
TI Pressure measurements using hybrid femtosecond/picosecond rotational
coherent anti-Stokes Raman scattering
SO OPTICS LETTERS
LA English
DT Article
ID LASER-INDUCED FLUORESCENCE; GAS-PHASE THERMOMETRY; RAYLEIGH-SCATTERING;
CARS MEASUREMENTS; SPECTROSCOPY; TEMPERATURE; LINEWIDTHS; VELOCITY; SHOT
AB We investigate the feasibility of gas-phase pressure measurements using fs/ps rotational CARS. Femtosecond pump and Stokes pulses impulsively prepare a rotational Raman coherence, which is probed by a high-energy 5-ps pulse introduced at a time delay from the Raman preparation. These ultrafast laser pulses are shorter than collisional-dephasing time scales, enabling a new hybrid time- and frequency-domain detection scheme for pressure. Single-laser-shot rotational CARS spectra were recorded from N-2 contained in a room-temperature gas cell for pressures from 0.4 to 3 atm and probe delays ranging from 16 to 298 ps. Sensitivity of the accuracy and precision of the pressure data to probe delay was investigated. The technique exhibits superior precision and comparable accuracy to previous laser-diagnostic pressure measurements.
C1 [Kearney, Sean P.] Sandia Natl Labs, Engn Sci Ctr, Albuquerque, NM 87185 USA.
[Danehy, Paul M.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Kearney, SP (reprint author), Sandia Natl Labs, Engn Sci Ctr, POB 5800, Albuquerque, NM 87185 USA.
EM spkearn@sandia.gov
FU NASA Langley Research Center's Internal Research and Development (IRAD)
Program; U.S. Department of Energy (DOE) [DE-AC04-94AL85000]; Sandia
National Laboratories
FX NASA Langley Research Center's Internal Research and Development (IRAD)
Program; U.S. Department of Energy (DOE) (DE-AC04-94AL85000); Sandia
National Laboratories.
NR 17
TC 0
Z9 0
U1 2
U2 16
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
EI 1539-4794
J9 OPT LETT
JI Opt. Lett.
PD SEP 1
PY 2015
VL 40
IS 17
BP 4082
EP 4085
DI 10.1364/OL.40.004082
PG 4
WC Optics
SC Optics
GA CQ7UM
UT WOS:000360810200041
PM 26368717
ER
PT J
AU Nadeau, JL
Cho, YB
Lindensmith, CA
AF Nadeau, Jay L.
Cho, Yong Bin
Lindensmith, Christian A.
TI Use of dyes to increase phase contrast for biological holographic
microscopy
SO OPTICS LETTERS
LA English
DT Article
ID PHOTODYNAMIC THERAPY; CELL MORPHOMETRY; REFRACTIVE-INDEX; LIVING CELLS;
PHOTOSENSITIZERS; ABSORPTION; PORPHYRINS
AB Holographic microscopy is an emerging biological technique that provides amplitude and quantitative phase imaging, though the contrast provided by many cell types and organelles is low, and until now no dyes were known that increased contrast. Here we show that the metallocorrole Ga(tpfc)(SO3H)(2), which has a strong Soret band absorption, increases contrast in both amplitude and phase and facilitates tracking of Escherichia coli with minimal toxicity. The change in phase contrast may be calculated from the dye-absorbance spectrum using the Kramers-Kronig relations, and represents a general principle that may be applied to any dye or cell type. This enables the use of holographic microscopy for all applications in which specific labeling is desired. (C) 2015 Optical Society of America
C1 [Nadeau, Jay L.; Cho, Yong Bin] CALTECH, Div Engn & Appl Sci, Grad Aerosp Labs, Pasadena, CA 91125 USA.
[Lindensmith, Christian A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nadeau, JL (reprint author), CALTECH, Div Engn & Appl Sci, Grad Aerosp Labs, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM jnadeau@caltech.edu
FU Gordon and Betty Moore Foundation [4037, 4038]
FX Gordon and Betty Moore Foundation (4037, 4038).
NR 28
TC 3
Z9 3
U1 1
U2 5
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
EI 1539-4794
J9 OPT LETT
JI Opt. Lett.
PD SEP 1
PY 2015
VL 40
IS 17
BP 4114
EP 4117
DI 10.1364/OL.40.004114
PG 4
WC Optics
SC Optics
GA CQ7UM
UT WOS:000360810200049
PM 26368725
ER
PT J
AU Berra, LM
Slaterb, JW
Olcmen, SM
AF Berra, Lee M.
Slaterb, John W.
Olcmen, Semih M.
TI Conceptual redesign of the B-1B bomber inlets for improved supersonic
performance
SO AEROSPACE SCIENCE AND TECHNOLOGY
LA English
DT Article
AB This paper presents a conceptual study of two alternative inlet concepts for the United States Air Force B-1B bomber to provide for improved supersonic performance with expansion of capabilities to high-altitude, high-speed flight at Mach 2.0. The two inlet concepts are two-dimensional, variable-ramp inlet systems designed to replace the current fixed-geometry, pitot inlets of the B-1B. One inlet incorporates a two-ramp system, while a second inlet incorporates a two-ramp system containing an isentropic contour. The entire inlet system including the supersonic diffuser, throat, cowl lip, and subsonic diffuser sections was designed to maximize the total pressure recovery at the engine fan face to achieve maximum thrust by the engine at Mach 2.0 conditions. Analytic methods implemented into the MATLAB and the NASA SUPIN codes are used to design and analyze the two-dimensional inlet concepts. In addition, WIND-US computational fluid dynamics simulations were used to check and improve the results of the analytic design methods. The results suggest that at Mach 2.0, the total pressure recovery of the inlets could increase from 0.70 to 0.94. The inlet capture area and cowl drag increased; however, the overall improvements resulted in a 98% thrust increase over the existing inlet at the design point. Published by Elsevier Masson SAS.
C1 [Berra, Lee M.] USAF Test Pilot Sch Class 15B, Edwards AFB, CA 93524 USA.
[Slaterb, John W.] NASA, John H Glenn Res Ctr, Inlet & Nozzle Branch, Cleveland, OH 44135 USA.
[Olcmen, Semih M.] Univ Alabama, Dept Aerosp Engn & Mech, Tuscaloosa, AL 35487 USA.
RP Berra, LM (reprint author), USAF Test Pilot Sch Class 15B, 220 South Wolfe Ave, Edwards AFB, CA 93524 USA.
EM Lee.Berra@gmail.com; john.w.slater@nasa.gov; Solcmen@eng.ua.edu
OI Olcmen, Semih/0000-0001-8272-3912
NR 12
TC 0
Z9 0
U1 2
U2 8
PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER
PI PARIS
PA 23 RUE LINOIS, 75724 PARIS, FRANCE
SN 1270-9638
EI 1626-3219
J9 AEROSP SCI TECHNOL
JI Aerosp. Sci. Technol.
PD SEP
PY 2015
VL 45
BP 476
EP 483
DI 10.1016/j.ast.2015.06.017
PG 8
WC Engineering, Aerospace
SC Engineering
GA CQ4TP
UT WOS:000360597800051
ER
PT J
AU Yue, P
Ramachandran, R
Baumann, P
AF Yue, Peng
Ramachandran, Rahul
Baumann, Peter
TI Editorial: intelligent GIServices
SO EARTH SCIENCE INFORMATICS
LA English
DT Editorial Material
C1 [Yue, Peng] Wuhan Univ, State Key Lab Informat Engn Surveying Mapping & R, Wuhan 430079, Hubei, Peoples R China.
[Ramachandran, Rahul] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Baumann, Peter] Jacobs Univ Bremen, D-28759 Bremen, Germany.
RP Yue, P (reprint author), Wuhan Univ, State Key Lab Informat Engn Surveying Mapping & R, 129 Luoyu Rd, Wuhan 430079, Hubei, Peoples R China.
EM pyue@whu.edu.cn
NR 5
TC 0
Z9 0
U1 4
U2 12
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
EI 1865-0481
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD SEP
PY 2015
VL 8
IS 3
SI SI
BP 461
EP 462
DI 10.1007/s12145-015-0237-z
PG 2
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA CQ6CW
UT WOS:000360693000001
ER
PT J
AU Whitehall, K
Mattmann, CA
Jenkins, G
Rwebangira, M
Demoz, B
Waliser, D
Kim, J
Goodale, C
Hart, A
Ramirez, P
Joyce, MJ
Boustani, M
Zimdars, P
Loikith, P
Lee, H
AF Whitehall, Kim
Mattmann, Chris A.
Jenkins, Gregory
Rwebangira, Mugizi
Demoz, Belay
Waliser, Duane
Kim, Jinwon
Goodale, Cameron
Hart, Andrew
Ramirez, Paul
Joyce, Michael J.
Boustani, Maziyar
Zimdars, Paul
Loikith, Paul
Lee, Huikyo
TI Exploring a graph theory based algorithm for automated identification
and characterization of large mesoscale convective systems in satellite
datasets
SO EARTH SCIENCE INFORMATICS
LA English
DT Article
DE Mesoscale convective systems; Mesoscale convective complexes; Graph
theory; Infrared satellite dataset; Precipitation satellite-based
dataset
ID CLOUD CLUSTERS; DIURNAL-VARIATIONS; EASTERLY WAVES; ATLANTIC-OCEAN;
WEST-AFRICA; LIFE-CYCLE; TRACKING; COMPLEXES; THUNDERSTORMS; METHODOLOGY
AB Mesoscale convective systems are high impact convectively driven weather systems that contribute large amounts to the precipitation daily and monthly totals at various locations globally. As such, an understanding of the lifecycle, characteristics, frequency and seasonality of these convective features is important for several sectors and studies in climate studies, agricultural and hydrological studies, and disaster management. This study explores the applicability of graph theory to creating a fully automated algorithm for identifying mesoscale convective systems and determining their precipitation characteristics from satellite datasets. Our results show that applying graph theory to this problem allows for the identification of features from infrared satellite data and the seamlessly identification in a precipitation rate satellite-based dataset, while innately handling the inherent complexity and non-linearity of mesoscale convective systems.
C1 [Whitehall, Kim; Jenkins, Gregory; Rwebangira, Mugizi; Demoz, Belay] Howard Univ, Washington, DC 20059 USA.
[Whitehall, Kim; Mattmann, Chris A.; Waliser, Duane; Goodale, Cameron; Hart, Andrew; Ramirez, Paul; Joyce, Michael J.; Boustani, Maziyar; Zimdars, Paul; Loikith, Paul; Lee, Huikyo] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Mattmann, Chris A.] Univ So Calif, Los Angeles, CA USA.
[Waliser, Duane; Kim, Jinwon] Univ Calif Los Angeles, Joint Inst Reg & Earth Syst Sci Engn, Los Angeles, CA USA.
RP Mattmann, CA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM mattmann@usc.edu
FU NASA Jet Propulsion Laboratory Regional Climate Model Evaluation System
(RCMES); Apache Open Climate Workbench (Apache OCW)
FX We acknowledge the NASA GES DISC as the data source. The authors wish to
thank the NASA Jet Propulsion Laboratory Regional Climate Model
Evaluation System (RCMES) and the Apache Open Climate Workbench (Apache
OCW) teams for their support. The authors also wish to thank the reviews
for their comments that improved the quality of the article.
NR 36
TC 1
Z9 1
U1 4
U2 5
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
EI 1865-0481
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD SEP
PY 2015
VL 8
IS 3
SI SI
BP 663
EP 675
DI 10.1007/s12145-014-0181-3
PG 13
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA CQ6CW
UT WOS:000360693000016
ER
PT J
AU Liu, Z
Moore, AW
Owen, S
AF Liu, Zhen
Moore, Angelyn W.
Owen, Susan
TI Recurrent slow slip event reveals the interaction with seismic slow
earthquakes and disruption from large earthquake
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Time-series analysis; Satellite geodesy; Transient deformation;
Subduction zone processes
ID LOW-FREQUENCY EARTHQUAKES; TOHOKU-OKI EARTHQUAKE; NON-VOLCANIC TREMOR;
SOUTHWEST JAPAN; NANKAI TROUGH; BUNGO CHANNEL; SUBDUCTION ZONE;
SAN-ANDREAS; SILENT SLIP; GPS DATA
AB It remains enigmatic how slow slip events (SSEs) interact with other slow seismic events and large distant earthquakes at many subduction zones. Here we model the spatiotemporal slip evolution of the most recent long-term SSE in 2009-2011 in the Bungo Channel region, southwest Japan using GEONET GPS position time-series and a Kalman filter-based, time-dependent slip inversion method. We examine the space-time relationship between the geodetically determined slow slip transient and seismically observed low frequency earthquakes (LFEs) and very-low frequency earthquakes (V-LFEs) near the Nankai trough. We find a strong but distinct temporal correlation between transient slip and LFEs and V-LFEs, suggesting a different relationship to the SSE. We also find the great Tohoku-Oki earthquake appears to disrupt the normal source process of the SSE, probably reflecting large-scale stress redistribution caused by the earthquake. Comparison of the 2009-2011 SSE with others in the same region shows much similarity in slip and moment release, confirming its recurrent nature. Comparison of transient slip with plate coupling shows that slip transients mainly concentrate on the transition zone from strong coupling region to downdip LFEs with transient slip relieving elastic strain accumulation at transitional depth. The less consistent spatial correlation between the long-term SSE and seismic slow earthquakes, and susceptibility of these slow earthquakes to various triggering sources including long-term slow slip, suggests caution in using the seismically determined slow earthquakes as a proxy for slow slip.
C1 [Liu, Zhen; Moore, Angelyn W.; Owen, Susan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Liu, Z (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM zhen.liu@jpl.nasa.gov
RI Liu, Zhen/D-8334-2017
FU National Aeronautics and Space Administration at the Jet Propulsion
Laboratory, California Institute of Technology
FX Precise GPS orbit products used for time-series analysis were provided
by JPL GPS Analysis Centre. All original GEONET RINEX data provided to
Caltech by the Geospatial Information Authority (GSI) of Japan. We thank
Youichi Asano for sending us the V-LFE catalogue in their published
paper. Reviews by two anonymous reviewers helped improve the manuscript.
We are grateful to Japan Meteorological Agency for the LFE hypocentre
data. The research described in this paper was supported under the
contract with the National Aeronautics and Space Administration at the
Jet Propulsion Laboratory, California Institute of Technology.
NR 55
TC 1
Z9 1
U1 4
U2 12
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 SEP
PY 2015
VL 202
IS 3
BP 1555
EP 1565
DI 10.1093/gji/ggv238
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CQ5EG
UT WOS:000360625500009
ER
PT J
AU Reuveni, Y
Bock, Y
Tong, XP
Moore, AW
AF Reuveni, Yuval
Bock, Yehuda
Tong, Xiaopeng
Moore, Angelyn W.
TI Calibrating interferometric synthetic aperture radar (InSAR) images with
regional GPS network atmosphere models
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Satellite geodesy; Radar interferometry; Ionosphere; atmosphere
interactions
ID SAN-ANDREAS FAULT; INTERSEISMIC STRAIN; DEFORMATION; EARTHQUAKE;
CALIFORNIA; ERRORS; MAPS; INTERFEROGRAMS; ACCUMULATION; SURFACE
AB Interferometric synthetic aperture radar (InSAR) technology provides a valuable tool for obtaining Earth surface deformation and topography at high spatial resolution for crustal deformation studies. Similar to global positioning system (GPS), InSAR measurements are affected by the Earth's ionospheric and tropospheric layers as the electromagnetic signals significantly refract while propagating through the different layers. While GPS signals propagating through the neutral atmosphere are affected primarily by the distribution, pressure and temperature of atmospheric gases, including water vapour, the propagation through the ionosphere is mainly affected by the number of free electrons along the signal path. Here, we present the use of dense regional GPS networks for extracting tropospheric zenith delays and ionospheric total electron content (TEC) maps in order to reduce the noise levels in InSAR images. The results show significant reduction in the root mean square (RMS) values when simultaneously combining the two corrections, both at short time periods where no surface deformation is expected, and at longer periods, where imaging of localized subsidence and fault creep is enhanced.
C1 [Reuveni, Yuval; Bock, Yehuda; Tong, Xiaopeng] Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, La Jolla, CA 92093 USA.
[Reuveni, Yuval] Ariel Univ, Samaria & Jordan Rift Reg R&D Ctr, Ariel, Israel.
[Tong, Xiaopeng] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Moore, Angelyn W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Reuveni, Y (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, La Jolla, CA 92093 USA.
EM yreuveni@ucsd.edu
FU NASA-ROSES MEaSUREs grant [NNX13AI45A-001]; NSF grant [EAR-0323309]; NAS
[ESTO/AIST-11 NNX12AH55G]; ROSES [NNX12AK24G]; NSF EarthScope
[EAR-1252186]; Southern California Earthquake Center [12083]
FX Continuous GPS data were provided by SCIGN operated by the Scripps Orbit
and Permanent Array Center (SOPAC) under NASA-ROSES MEaSUREs grant
NNX13AI45A-001 and the U.S. Geological Survey, Pasadena, and by the
Plate Boundary Observatory (PBO) operated by UNAVCO for Earth-Scope
(http://www.earthscope.org) and supported by NSF grant EAR-0323309. This
work was funded by NASA grants ESTO/AIST-11 NNX12AH55G and ROSES
NNX12AK24G, NSF EarthScope Grant EAR-1252186, and Southern California
Earthquake Center award 12083. A portion of this work was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration. We
would like to thank Dr Zhen Liu from Jet Propulsion Laboratory for his
help with processing the raw ENVISAT data, suggestions and comments,
discussions with Dr Jianghui Geng at Scripps Institution of
Oceanography, and assistance from SOPAC staff including Mindy Squibb,
Anne Sullivan and Peng Fang.
NR 74
TC 1
Z9 1
U1 0
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 SEP
PY 2015
VL 202
IS 3
BP 2106
EP 2119
DI 10.1093/gji/ggv253
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CQ5EG
UT WOS:000360625500043
ER
PT J
AU Holzmann, GJ
AF Holzmann, Gerard J.
TI Code Evasion
SO IEEE SOFTWARE
LA English
DT Editorial Material
C1 Jet Prop Lab, Dev Stronger Methods Software Anal Code Review &, Pasadena, CA 91109 USA.
RP Holzmann, GJ (reprint author), Jet Prop Lab, Dev Stronger Methods Software Anal Code Review &, Pasadena, CA 91109 USA.
EM gholzmann@acm.org
NR 5
TC 0
Z9 0
U1 0
U2 1
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0740-7459
EI 1937-4194
J9 IEEE SOFTWARE
JI IEEE Softw.
PD SEP-OCT
PY 2015
VL 32
IS 5
BP 77
EP 80
PG 4
WC Computer Science, Software Engineering
SC Computer Science
GA CQ5OQ
UT WOS:000360655300014
ER
PT J
AU Gonzalez-Ovejero, D
Maci, S
AF Gonzalez-Ovejero, David
Maci, Stefano
TI Gaussian Ring Basis Functions for the Analysis of Modulated Metasurface
Antennas
SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION
LA English
DT Article
DE Basis functions; leaky-wave antennas; metasurfaces (MTSs); method of
moments (MoM); spectral-domain approach
ID LUNEBURG LENS ANTENNA; ELECTROMAGNETIC SCATTERING; TRANSFORMATION
ELECTROMAGNETICS; INTEGRAL-EQUATIONS; IMPEDANCE SURFACES;
GREENS-FUNCTIONS; METAMATERIALS; WAVES; MEDIA
AB This paper presents a novel type of basis functions, whose spectral-and space-domain properties can be exploited for the efficient method of moments (MoM) analysis of planar metasurface (MTS) antennas. The effect of the homogenized MTS is introduced in the integral equation as an impedance boundary condition (IBC). The proposed basis functions are shaped as Gaussian-type rings with small width and linear azimuthal phase. The analytical form of the spectrum of the Gaussian ring basis allows for a closed-form evaluation of the MoM impedance matrix's entries. Moreover, these basis functions account for the global evolution of the surface current density in an effective manner, reducing the size of the MoM system of equations with respect to the case of subdomain basis functions. These features allow one to carry out a direct solution for problems with a diameter of up to 15 wavelengths in less than 1 min using a conventional laptop. The applicability on practical antennas has been tested through the full-wave analysis of MTS antennas implemented with small printed elements.
C1 [Gonzalez-Ovejero, David; Maci, Stefano] Univ Siena, Dept Informat Engn & Math, I-53100 Siena, Italy.
[Gonzalez-Ovejero, David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gonzalez-Ovejero, D (reprint author), Univ Siena, Dept Informat Engn & Math, Via Laterina 8, I-53100 Siena, Italy.
EM david.gonzalez@jpl.nasa.gov; macis@dii.unisi.it
OI Gonzalez Ovejero, David/0000-0002-2552-0649
FU European Space Agency (ESA-ESTEC, Noordwijk, The Netherlands)
[AO/1-7069/12/NL/MH]; U.S. Army Research Laboratory through USAIT-CA
[W911NF-13-1-0454]; Marie Curie International Outgoing Fellowship within
European Community; National Aeronautics and Space Administration (NASA)
FX This work was supported in part by the European Space Agency (ESA-ESTEC,
Noordwijk, The Netherlands) under contract AO/1-7069/12/NL/MH and in
part by the U.S. Army Research Laboratory through USAIT-CA, under
contract W911NF-13-1-0454. The work of D. Gonzalez-Ovejero was supported
by a Marie Curie International Outgoing Fellowship within the 7th
European Community Framework Programme, and partly carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with National Aeronautics and Space Administration (NASA).
NR 35
TC 6
Z9 6
U1 7
U2 19
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-926X
EI 1558-2221
J9 IEEE T ANTENN PROPAG
JI IEEE Trans. Antennas Propag.
PD SEP
PY 2015
VL 63
IS 9
BP 3982
EP 3993
DI 10.1109/TAP.2015.2442585
PG 12
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA CQ7SE
UT WOS:000360803400021
ER
PT J
AU Naud, CM
Posselt, DJ
van den Heever, SC
AF Naud, Catherine M.
Posselt, Derek J.
van den Heever, Susan C.
TI A CloudSat-CALIPSO View of Cloud and Precipitation Properties across
Cold Fronts over the Global Oceans
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Clouds; Cold fronts; Fronts; Precipitation; Warm fronts
ID MIDLATITUDE CYCLONES; CIRCULATION SYSTEMS; ERA-INTERIM; WARM;
ORGANIZATION; SATELLITE; FEATURES; NORTHERN; STORMS; GCM
AB The distribution of cloud and precipitation properties across oceanic extratropical cyclone cold fronts is examined using four years of combined CloudSat radar and CALIPSO lidar retrievals. The global annual mean cloud and precipitation distributions show that low-level clouds are ubiquitous in the postfrontal zone while higher-level cloud frequency and precipitation peak in the warm sector along the surface front. Increases in temperature and moisture within the cold front region are associated with larger high-level but lower mid-/low-level cloud frequencies and precipitation decreases in the cold sector. This behavior seems to be related to a shift from stratiform to convective clouds and precipitation. Stronger ascent in the warm conveyor belt tends to enhance cloudiness and precipitation across the cold front. A strong temperature contrast between the warm and cold sectors also encourages greater post-cold-frontal cloud occurrence. While the seasonal contrasts in environmental temperature, moisture, and ascent strength are enough to explain most of the variations in cloud and precipitation across cold fronts in both hemispheres, they do not fully explain the differences between Northern and Southern Hemisphere cold fronts. These differences are better explained when the impact of the contrast in temperature across the cold front is also considered. In addition, these large-scale parameters do not explain the relatively large frequency in springtime postfrontal precipitation.
C1 [Naud, Catherine M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[Naud, Catherine M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Posselt, Derek J.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[van den Heever, Susan C.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
RP Naud, CM (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA.
EM cn2140@columbia.edu
RI van den Heever, Susan/E-8728-2011; Posselt, Derek/I-4912-2012
OI van den Heever, Susan/0000-0001-9843-3864; Posselt,
Derek/0000-0002-5670-5822
FU NASA CloudSat Science Team Recompete Grant [NNX13AQ33G]; NASA the
Science of Terra and Aqua Grant [NNX11AH22G]
FX The CloudSat-CALIPSO products were obtained from the CloudSat Data
Processing Center. The MERRA outputs were obtained from the Goddard
Earth Sciences Data and Information Services Center. The MCMS dataset,
documentation, and algorithm are available at
http://gcss-dime.giss.nasa.gov/mcms/. We thank Mike Bauer for the
ERA-Interimbased dataset. This work is funded by the NASA CloudSat
Science Team Recompete Grant NNX13AQ33G. CMN is also funded by NASA the
Science of Terra and Aqua Grant NNX11AH22G. We thank the editor and
three anonymous reviewers for helping us significantly improve this
manuscript.
NR 42
TC 5
Z9 5
U1 4
U2 13
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD SEP
PY 2015
VL 28
IS 17
BP 6743
EP 6762
DI 10.1175/JCLI-D-15-0052.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CQ4QW
UT WOS:000360590700009
ER
PT J
AU Kim, D
Ahn, MS
Kang, IS
Del Genio, AD
AF Kim, Daehyun
Ahn, Min-Seop
Kang, In-Sik
Del Genio, Anthony D.
TI Role of Longwave Cloud-Radiation Feedback in the Simulation of the
Madden-Julian Oscillation
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Madden-Julian oscillation; Longwave radiation; Climate models; Cloud
parameterizations; Intraseasonal variability
ID GENERAL-CIRCULATION MODEL; LARGE-SCALE MODELS; TEMPERATURE-GRADIENT
APPROXIMATION; TROPICAL INTRASEASONAL OSCILLATION; COMMUNITY ATMOSPHERE
MODEL; PHYSICALLY-BASED SCHEME; INCLUDING MASS FLUXES; STATIC ENERGY
BUDGET; CUMULUS PARAMETERIZATION; CLIMATE MODELS
AB The role of the cloud-radiation interaction in the simulation of the Madden-Julian oscillation (MJO) is investigated. A special focus is on the enhancement of column-integrated diabatic heating due to the greenhouse effects of clouds and moisture in the region of anomalous convection. The degree of this enhancement, the greenhouse enhancement factor (GEF), is measured at different precipitation anomaly regimes as the negative ratio of anomalous outgoing longwave radiation to anomalous precipitation.Observations show that the GEF varies significantly with precipitation anomaly and with the MJO cycle. The greenhouse enhancement is greater in weak precipitation anomaly regimes and its effectiveness decreases monotonically with increasing precipitation anomaly. The GEF also amplifies locally when convection is strengthened in association with the MJO, especially in the weak precipitation anomaly regime (<5 mm day(-1)).A robust statistical relationship is found among CMIP5 climate model simulations between the GEF and the MJO simulation fidelity. Models that simulate a stronger MJO also simulate a greater GEF, especially in the weak precipitation anomaly regime (<5 mm day(-1)). Models with a greater GEF in the strong precipitation anomaly regime (>30 mm day(-1)) represent a slightly slower MJO propagation speed. Many models that lack the MJO underestimate the GEF in general and in particular in the weak precipitation anomaly regime. The results herein highlight that the cloud-radiation interaction is a crucial process for climate models to correctly represent the MJO.
C1 [Kim, Daehyun] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Ahn, Min-Seop; Kang, In-Sik] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea.
[Del Genio, Anthony D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Kim, D (reprint author), Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
EM daehyun@uw.edu
RI 안, 민섭/D-9972-2015
FU NASA [NNX13AM18G]; Korea Meteorological Administration Research and
Development Program [CATER 2013-3142]; National Research Foundation of
Korea (NRF) - Korean government (MEST) [NRF-2012M1A2A2671775]; Brain
Korea 21 Plus; NASA Modeling and Analysis and Precipitation Measurement
Mission Programs
FX We thank Adam H. Sobel for his thoughtful comments on an earlier version
of the manuscript. D. Kim was supported by the NASA Grant NNX13AM18G and
the Korea Meteorological Administration Research and Development Program
under Grant CATER 2013-3142. M.-S. Ahn and I.-S. Kang were supported by
a National Research Foundation of Korea (NRF) grant funded by the Korean
government (MEST; NRF-2012M1A2A2671775) and by the Brain Korea 21 Plus.
A. D. Del Genio was supported by the NASA Modeling and Analysis and
Precipitation Measurement Mission Programs.
NR 93
TC 5
Z9 5
U1 1
U2 12
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD SEP
PY 2015
VL 28
IS 17
BP 6979
EP 6994
DI 10.1175/JCLI-D-14-00767.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CQ4QW
UT WOS:000360590700021
ER
PT J
AU Hoyt, D
AF Hoyt, Diana
TI Big Data: A Revolution that Will Transform How We Live, Work, and Think
SO RESEARCH-TECHNOLOGY MANAGEMENT
LA English
DT Book Review
C1 [Hoyt, Diana] NASA, Washington, DC USA.
[Hoyt, Diana] Congress, New York, NY USA.
[Hoyt, Diana] Congress Space Caucus, New York, NY USA.
RP Hoyt, D (reprint author), NASA, Strateg Partnerships Program, Washington, DC 20005 USA.
EM diana.hoyt@nasa.gov
NR 1
TC 0
Z9 0
U1 4
U2 26
PU INDUSTRIAL RESEARCH INST, INC
PI ARLINGTON
PA 2300 CLARENDON BLVD, STE 400, ARLINGTON, VA 22201 USA
SN 0895-6308
EI 1930-0166
J9 RES TECHNOL MANAGE
JI Res.-Technol. Manage.
PD SEP-OCT
PY 2015
VL 58
IS 5
BP 66
EP 67
PG 2
WC Business; Engineering, Industrial; Management
SC Business & Economics; Engineering
GA CQ7KH
UT WOS:000360782400014
ER
PT J
AU Adirosi, E
Baldini, L
Lombardo, F
Russo, F
Napolitano, F
Volpi, E
Tokay, A
AF Adirosi, E.
Baldini, L.
Lombardo, F.
Russo, F.
Napolitano, F.
Volpi, E.
Tokay, A.
TI Comparison of different fittings of drop spectra for rainfall retrievals
SO ADVANCES IN WATER RESOURCES
LA English
DT Article
DE Rainfall remote sensing; Drop size distribution; Tail behavior;
Disdrometer
ID RAINDROP-SIZE DISTRIBUTION; X-BAND; GAMMA-DISTRIBUTIONS; RADAR
MEASUREMENTS; CONVECTIVE CLOUDS; MOMENT ESTIMATORS; KINETIC-ENERGY;
PARAMETERS; PRECIPITATION; DISDROMETER
AB It is widely acknowledged that a thorough characterization of the raindrop size distribution (DSD) inay address many needs regarding the remote sensing of precipitation, which is central to new research challenges related to the estimation and management of water resources, in particular, the third and higher moments (up to the sixth) of DSD are proportional to relevant hydrological and meteorological parameters (i.e., rain rate, liquid water content, radar reflectivity, and kinetic energy). Therefore, the retrieval process of these quantities is usually based upon higher-order statistics that are mainly influenced by the upper part of the DSD (i.e., its tail behavior). In this study, we first investigate the effects on rainfall integral parameters of truncating the DSD at upper drop diameters when assuming heavy- and light-tailed distributions. Then, we compare both the tails (i.e., large drops only) and the entire empirical distributions of thousands of disdrometer-measured raindrop spectra with four common theoretical distributions characterized by different tail behaviors (i.e., heavy- and light-tailed distributions): the Pareto, lognormal, gamma, and Weibull distributions. In particular, we analyze the relative quality of each distribution (relative ranking) by means of a straightforward method. Observational data consist of 1-min spectra collected by two-dimensional video disdrometers (2DVD) during three pre-launch field campaigns of the NASA Global Precipitation Measurement (GPM) mission located in (i) Rome (HyMeX SOP 1, (ii) Central Oklahoma (MC3E,), and (iii) Eastern Iowa (IFloodS). The results obtained from the analysis of the three datasets were consistent with each other, and they show that the lighter-tailed distributions are in better agreement with the observed size spectra than the heavier-tailed distributions. However, we also found significant departures of empirical drop spectra from light-tailed distributions, especially when fitting only the tail of the distributions. These departures may imply a dramatic increase of uncertainty in the statistical estimation of high-order DSD moments, thus making the retrieval process unreliable. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Adirosi, E.; Baldini, L.] Natl Res Council Italy CNR, Inst Atmospher Sci & Climate ISAC, Area Ricerca Roma Tor Vergata 2, I-00133 Rome, Italy.
[Adirosi, E.; Russo, F.; Napolitano, F.] Univ Roma La Sapienza, Dipartirnen Ingn Civile Edife & Ambientale, I-00185 Rome, Italy.
[Lombardo, F.; Volpi, E.] Univ Roma Tre, Dipartimento Ingn, Rome, Italy.
[Tokay, A.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Tokay, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Adirosi, E (reprint author), Natl Res Council Italy CNR, Inst Atmospher Sci & Climate ISAC, Area Ricerca Roma Tor Vergata 2, Via Foss Cavatiere 100, I-00133 Rome, Italy.
EM elisa.adirosi@artov.isac.cnr.it
RI Measurement, Global/C-4698-2015;
OI Baldini, Luca/0000-0001-5217-1205; Volpi, Elena/0000-0002-9511-1496;
Russo, Fabio/0000-0002-8153-9010; Lombardo, Federico/0000-0002-1772-0309
FU Italian Department of Civil Protection; NASA; Italian Ministry of
University and Research [PRIN 20102AXKAJ]
FX This research was partially supported by the Italian Department of Civil
Protection and NASA Precipitation Measurement Mission (PMM) under Ramesh
Kakar, program scientist, NASA Headquarters. The authors acknowledge the
anonymous reviewers for their detailed and helpful comments to the
manuscript. The authors acknowledge the NASA GPM mission ground
validation program under Matthew Schvvaller, GPM ground validation
manager, and Walter A. Petersen, GPM ground validation science manager,
for providing 2DVD data and contributions to the HyMeX field campaign.
Acknowledgments extend to the HyMeX program which this work is part of
Federico Lombardo and Elena Volpi acknowledge partial financial support
from the Italian Ministry of University and Research through the project
PRIN 20102AXKAJ.
NR 66
TC 6
Z9 6
U1 7
U2 16
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0309-1708
EI 1872-9657
J9 ADV WATER RESOUR
JI Adv. Water Resour.
PD SEP
PY 2015
VL 83
BP 55
EP 67
DI 10.1016/j.advwatres.2015.05.009
PG 13
WC Water Resources
SC Water Resources
GA CP9CV
UT WOS:000360192200006
ER
PT J
AU Willis, PA
Creamer, JS
Mora, MF
AF Willis, Peter A.
Creamer, Jessica S.
Mora, Maria F.
TI Implementation of microchip electrophoresis instrumentation for future
spaceflight missions
SO ANALYTICAL AND BIOANALYTICAL CHEMISTRY
LA English
DT Review
DE Capillary electrophoresis/electrophoresis;
Microfluidics/microfabrication; Organic compounds/trace organic
compounds; Separations/instrumentation; Technology readiness level;
Systems engineering
ID MARS ORGANIC ANALYZER; NONAQUEOUS CAPILLARY-ELECTROPHORESIS; POLYCYCLIC
AROMATIC-HYDROCARBON; NEUTRAL MASS-SPECTROMETER;
POLYMERASE-CHAIN-REACTION; IN-SITU ANALYSIS; AMINO-ACIDS; INTERNAL
STRUCTURE; TITANS ATMOSPHERE; MEMBRANE VALVES
AB We present a comprehensive discussion of the role that microchip electrophoresis (ME) instrumentation could play in future NASA missions of exploration, as well as the current barriers that must be overcome to make this type of chemical investigation possible. We describe how ME would be able to fill fundamental gaps in our knowledge of the potential for past, present, or future life beyond Earth. Despite the great promise of ME for ultrasensitive portable chemical analysis, to date, it has never been used on a robotic mission of exploration to another world. We provide a current snapshot of the technology readiness level (TRL) of ME instrumentation, where the TRL is the NASA systems engineering metric used to evaluate the maturity of technology, and its fitness for implementation on missions. We explain how the NASA flight implementation process would apply specifically to ME instrumentation, and outline the scientific and technology development issues that must be addressed for ME analyses to be performed successfully on another world. We also outline research demonstrations that could be accomplished by independent researchers to help advance the TRL of ME instrumentation for future exploration missions. The overall approach described here for system development could be readily applied to a wide range of other instrumentation development efforts having broad societal and commercial impact.
C1 [Willis, Peter A.; Creamer, Jessica S.; Mora, Maria F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Willis, PA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM peter.a.willis@jpl.nasa.gov
RI Mora, Maria/C-9753-2009
FU Planetary Instrument Concepts for the Advancement of Solar System
Observations (PICASSO) program; NASA Postdoctoral Program at the Jet
Propulsion Laboratory
FX This review was written at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration (NASA). Financial support was provided by the
Planetary Instrument Concepts for the Advancement of Solar System
Observations (PICASSO) program and the NASA Postdoctoral Program at the
Jet Propulsion Laboratory, administered by Oak Ridge Associated
Universities through a contract with NASA. Nathan Bramall of Los Gatos
Research designed and fabricated the majority of the original Chemical
Laptop hardware and software subsystem elements in collaboration with
the Jet Propulsion Laboratory. Chuck Bryson developed the hardware for
the subcritical water extraction instrument used for our 2005 Atacama
Desert field campaign. Greg Borowski developed the PISCES CADmodel. Andy
Spry provided helpful input on planetary protection and contamination
control issues. We thank Curt Henry for helpful discussions and comments
regarding the application of systems engineering approaches for in situ
instrument development, and Sabrina Feldman and Chris Webster for
ongoing guidance and support.
NR 155
TC 4
Z9 4
U1 4
U2 27
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1618-2642
EI 1618-2650
J9 ANAL BIOANAL CHEM
JI Anal. Bioanal. Chem.
PD SEP
PY 2015
VL 407
IS 23
BP 6939
EP 6963
DI 10.1007/s00216-015-8903-z
PG 25
WC Biochemical Research Methods; Chemistry, Analytical
SC Biochemistry & Molecular Biology; Chemistry
GA CQ2EL
UT WOS:000360412100005
PM 26253225
ER
PT J
AU Abedin, MN
Bradley, AT
Sharma, SK
Misra, AK
Lucey, PG
Mckay, CP
Ismail, S
Sandford, SP
AF Abedin, M. Nurul
Bradley, Arthur T.
Sharma, Shiv K.
Misra, Anupam K.
Lucey, Paul G.
Mckay, Christopher P.
Ismail, Syed
Sandford, Stephen P.
TI Mineralogy and astrobiology detection using laser remote sensing
instrument
SO APPLIED OPTICS
LA English
DT Article
ID INDUCED BREAKDOWN SPECTROSCOPY; RAMAN-SPECTROSCOPY; PLANETARY SURFACES;
MOJAVE DESERT; GALE CRATER; CARBONATE; EUROPA; SULFUR; ROCKS; MISSIONS
AB A multispectral instrument based on Raman, laser-induced fluorescence (LIF), laser-induced breakdown spectroscopy (LIBS), and a lidar system provides high-fidelity scientific investigations, scientific input, and science operation constraints in the context of planetary field campaigns with the Jupiter Europa Robotic Lander and Mars Sample Return mission opportunities. This instrument conducts scientific investigations analogous to investigations anticipated for missions to Mars and Jupiter's icy moons. This combined multispectral instrument is capable of performing Raman and fluorescence spectroscopy out to a >100 m target distance from the rover system and provides single-wavelength atmospheric profiling over long ranges (>20 km). In this article, we will reveal integrated remote Raman, LIF, and lidar technologies for use in robotic and lander-based planetary remote sensing applications. Discussions are focused on recently developed Raman, LIF, and lidar systems in addition to emphasizing surface water ice, surface and subsurface minerals, organics, biogenic, biomarker identification, atmospheric aerosols and clouds distributions, i.e., near-field atmospheric thin layers detection for next robotic-lander based instruments to measure all the above-mentioned parameters.
C1 [Abedin, M. Nurul; Bradley, Arthur T.] NASA Langley Res Ctr, Remote Sensing Flight Syst Branch, Hampton, VA 23681 USA.
[Sharma, Shiv K.; Misra, Anupam K.; Lucey, Paul G.] Univ Hawaii, HIGP, Honolulu, HI 96822 USA.
[Mckay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Ismail, Syed] NASA Langley Res Ctr, Atmospher Chem & Dynam Branch, Hampton, VA 23681 USA.
[Sandford, Stephen P.] NASA Langley Res Ctr, Space Technol & Explorat Directorate, Hampton, VA 23681 USA.
RP Abedin, MN (reprint author), NASA Langley Res Ctr, Remote Sensing Flight Syst Branch, 5 N Dryden St,MS 468, Hampton, VA 23681 USA.
EM m.n.abedin@nasa.gov
FU NASA Mars Instrument Development Project; NASA EPSCoR; NASA LaRC
FX NASA Mars Instrument Development Project; NASA EPSCoR to the University
of Hawaii; NASA LaRC.
NR 61
TC 4
Z9 4
U1 5
U2 33
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 SEP 1
PY 2015
VL 54
IS 25
BP 7598
EP 7611
DI 10.1364/AO.54.007598
PG 14
WC Optics
SC Optics
GA CQ1GB
UT WOS:000360344200021
PM 26368883
ER
PT J
AU Nieth, A
Verseux, C
Barnert, S
Suss, R
Romer, W
AF Nieth, Anita
Verseux, Cyprien
Barnert, Sabine
Suess, Regine
Roemer, Winfried
TI A first step toward liposome-mediated intracellular bacteriophage
therapy
SO EXPERT OPINION ON DRUG DELIVERY
LA English
DT Article
DE antibiotic resistance; bacteriophage therapy; intracellular pathogens;
liposomes trafficking; tuberculosis
ID PHAGE THERAPY; MYCOBACTERIUM-TUBERCULOSIS; NONVIRULENT MYCOBACTERIUM;
LIPID VESICLES; DRUG-DELIVERY; IN-VIVO; ENCAPSULATION; AVIUM;
MICROENCAPSULATION; INFECTION
AB Objectives: The emergence of antibiotic-resistant bacteria presents a severe challenge to medicine and public health. While bacteriophage therapy is a promising alternative to traditional antibiotics, the general inability of bacteriophages to penetrate eukaryotic cells limits their use against resistant bacteria, causing intracellular diseases like tuberculosis. Bacterial vectors show some promise in carrying therapeutic bacteriophages into cells, but also bring a number of risks like an overload of bacterial antigens or the acquisition of virulence genes from the pathogen.
Methods: As a first step in the development of a non-bacterial vector for bacteriophage delivery into pathogen-infected cells, we attempted to encapsulate bacteriophages into liposonnes.
Results: Here we report effective encapsulation of the model bacteriophage lambda eyfp and the mycobacteriophage TM4 into giant liposomes. Furthermore, we show that liposome-associated bacteriophages are taken up into eukaryotic cells more efficiently than free bacteriophages.
Conclusion: These are important milestones in the development of an intracellular bacteriophage therapy that might be useful in the fight against multi-drug-resistant intracellular pathogens like Mycobacterium tuberculosis.
C1 [Nieth, Anita; Roemer, Winfried] Univ Freiburg, Inst Biol 2, D-79104 Freiburg, Germany.
[Nieth, Anita; Roemer, Winfried] Univ Freiburg, Spemann Grad Sch Biol & Med SGBM, D-79104 Freiburg, Germany.
[Nieth, Anita; Roemer, Winfried] Univ Freiburg, BIOSS Ctr Biol Signalling Studies, D-79104 Freiburg, Germany.
[Verseux, Cyprien] Univ Roma Tor Vergata, Dept Biol, I-00133 Rome, Italy.
[Verseux, Cyprien] NASA, Ames Res Ctr, Educ Associates Program, Moffett Field, CA 94035 USA.
[Barnert, Sabine; Suess, Regine] Univ Freiburg, Dept Pharmaceut Technol & Biopharm, D-79104 Freiburg, Germany.
RP Romer, W (reprint author), Univ Freiburg, Inst Biol 2, Schanzlestr 1, D-79104 Freiburg, Germany.
EM anita_nieth@gmx.de; winfried.roemer@bioss.uni-freiburg.de
FU Excellence Initiative of the German Research Foundation (GSC 4, Spemann
Graduate School and EXC 294, BIOSS - Centre for Biological Signaling
Studies); Research Innovation Fund of the University of Freiburg
FX This study was supported by the Excellence Initiative of the German
Research Foundation (GSC 4, Spemann Graduate School and EXC 294, BIOSS -
Centre for Biological Signaling Studies) and the Research Innovation
Fund of the University of Freiburg. The authors have no other relevant
affiliations or financial involvement with any organization or entity
with a financial interest in or financial conflict with the subject
matter or materials discussed in the manuscript. This includes
employment, consultancies, honoraria, stock ownership or options, expert
testimony, grants or patents received or pending, or royalties.
NR 57
TC 2
Z9 3
U1 5
U2 45
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 1742-5247
EI 1744-7593
J9 EXPERT OPIN DRUG DEL
JI Expert Opin. Drug Deliv.
PD SEP
PY 2015
VL 12
IS 9
BP 1411
EP 1424
DI 10.1517/17425247.2015.1043125
PG 14
WC Pharmacology & Pharmacy
SC Pharmacology & Pharmacy
GA CP8ZV
UT WOS:000360184400003
PM 25937143
ER
PT J
AU Ting, DZY
Soibel, A
Hoglund, L
Gunapala, SD
AF Ting, David Z. -Y.
Soibel, Alexander
Hoeglund, Linda
Gunapala, Sarath D.
TI Theoretical Aspects of Minority Carrier Extraction in Unipolar Barrier
Infrared Detectors
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article; Proceedings Paper
CT US Workshop on the Physics and Chemistry of II-VI Materials
CY OCT 20-23, 2014
CL Baltimore, MD
SP US Army RDECOM CERDEC Night Vision & Elect Sensors Directorate, US Army Res Lab, US Army SMDC, Penn State Univ, US Navy Electro-Opt Ctr, Off Naval Res, AF Res Lab, Army Res Off, Minerals, Metal & Mat Soc
DE Infrared detector; type-II superlattice; unipolar barrier;
mid-wavelength infrared; long-wavelength infrared
ID NUMERICAL-SIMULATION; PHOTODETECTORS; SUPERLATTICES; DEVICES; HGCDTE
AB We have examined, theoretically, minority carrier collection in unipolar barrier infrared photodetectors. In barrier infrared detectors, for example the nBn, the unipolar barrier should block only majority carriers and allow unimpeded flow of minority carriers. However, an imperfect barrier would also block minority carriers, resulting in higher than expected turn-on bias. Minority carrier blocking can be caused by barrier doping or unintended band offset between the barrier and the absorber. The distinct manner in which these two mechanisms affect device performance were investigated. We found that introduction of an appropriate amount of barrier doping can reduce depletion dark current without increasing turn-on bias. We examined the effects of band structure on conductivity effective masses when the n-type absorber was a type-II superlattice (T2SL). We showed that for a long-wavelength infrared InAs/GaSb T2SL the vertical conductivity hole effective mass can be much smaller than that predicted by the simple band-edge effect mass picture, implying that the vertical hole mobility estimated from the band-edge effective mass can be unduly pessimistic.
C1 [Ting, David Z. -Y.; Soibel, Alexander; Hoeglund, Linda; Gunapala, Sarath D.] CALTECH, NASA, Jet Prop Lab, Ctr Infrared Photodetectors, Pasadena, CA 91109 USA.
[Ting, David Z. -Y.] Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ting, DZY (reprint author), CALTECH, NASA, Jet Prop Lab, Ctr Infrared Photodetectors, Pasadena, CA 91109 USA.
EM david.z.ting@jpl.nasa.gov
NR 44
TC 4
Z9 4
U1 5
U2 24
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
EI 1543-186X
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD SEP
PY 2015
VL 44
IS 9
BP 3036
EP 3043
DI 10.1007/s11664-015-3756-y
PG 8
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA CQ0TX
UT WOS:000360311300013
ER
PT J
AU Sullivan, W
Beck, J
Scritchfield, R
Skokan, M
Mitra, P
Sun, XL
Abshire, J
Carpenter, D
Lane, B
AF Sullivan, William, III
Beck, Jeffrey
Scritchfield, Richard
Skokan, Mark
Mitra, Pradip
Sun, Xiaoli
Abshire, James
Carpenter, Darren
Lane, Barry
TI Linear-Mode HgCdTe Avalanche Photodiodes for Photon-Counting
Applications
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article; Proceedings Paper
CT US Workshop on the Physics and Chemistry of II-VI Materials
CY OCT 20-23, 2014
CL Baltimore, MD
SP US Army RDECOM CERDEC Night Vision & Elect Sensors Directorate, US Army Res Lab, US Army SMDC, Penn State Univ, US Navy Electro-Opt Ctr, Off Naval Res, AF Res Lab, Army Res Off, Minerals, Metal & Mat Soc
DE Avalanche photodiode; HgCdTe; single-photon counting; mid-wave infrared;
photon detection efficiency; false-event rate
AB An overview of recent improvements in our understanding of, and the maturity of, linear-mode photon counting with the HgCdTe electron-initiated avalanche photodiode is presented. In 2010 DRS fabricated an experimental 2 x 8 array with (64 mu m)(2) pixels which enabled, for the first time, linear-mode photon counting by use of the MWIR cutoff HgCdTe electron-initiated avalanche photodiode. The device had a high single-photon signal-to-noise ratio of 13.7, an excess noise factor of 1.3-1.4, a 7 ns minimum time between events, and a broad spectral response extending from 0.4 mu m to 4.2 mu m. DRS recently fabricated a new set of devices with improved yield and performance compared with the first device: the false event rate was reduced by a factor of almost 10 to 150 kHz, the photon detection efficiency was increased from 50% to > 60%, and the APD gain was increased by a factor of 4 to over 1900.
C1 [Sullivan, William, III; Beck, Jeffrey; Scritchfield, Richard; Skokan, Mark; Mitra, Pradip] DRS Technol, Grp C4ISR, Dallas, TX 75243 USA.
[Sun, Xiaoli; Abshire, James] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Carpenter, Darren; Lane, Barry] A DIC Inc, Longwood, FL 32750 USA.
RP Sullivan, W (reprint author), DRS Technol, Grp C4ISR, 13544 N Cent Expressway, Dallas, TX 75243 USA.
EM billy.sullivan@drs.com
NR 5
TC 0
Z9 0
U1 2
U2 16
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
EI 1543-186X
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD SEP
PY 2015
VL 44
IS 9
BP 3092
EP 3101
DI 10.1007/s11664-015-3824-3
PG 10
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA CQ0TX
UT WOS:000360311300020
ER
PT J
AU Li, ZJ
McWilliams, JC
Ide, K
Farrara, JD
AF Li, Zhijin
McWilliams, James C.
Ide, Kayo
Farrara, John D.
TI A Multiscale Variational Data Assimilation Scheme: Formulation and
Illustration
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID RANGE FORECAST ERRORS; STATISTICAL STRUCTURE; RADIOSONDE DATA; ENSEMBLE
DATA; COVARIANCES; PREDICTION; SYSTEM
AB A multiscale data assimilation (MS-DA) scheme is formulated for fine-resolution models. A decomposition of the cost function is derived for a set of distinct spatial scales. The decomposed cost function allows for the background error covariance to be estimated separately for the distinct spatial scales, and multi-decorrelation scales to be explicitly incorporated in the background error covariance. MS-DA minimizes the partitioned cost functions sequentially from large to small scales. The multi-decorrelation length scale background error covariance enhances the spreading of sparse observations and prevents fine structures in high-resolution observations from being overly smoothed. The decomposition of the cost function also provides an avenue for mitigating the effects of scale aliasing and representativeness errors that inherently exist in a multiscale system, thus further improving the effectiveness of the assimilation of high-resolution observations. A set of one-dimensional experiments is performed to examine the properties of the MS-DA scheme. Emphasis is placed on the assimilation of patchy high-resolution observations representing radar and satellite measurements, alongside sparse observations representing those from conventional in situ platforms. The results illustrate how MS-DA improves the effectiveness of the assimilation of both these types of observations simultaneously.
C1 [Li, Zhijin] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[McWilliams, James C.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Ide, Kayo] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Ide, Kayo] Univ Maryland, Ctr Sci Computat & Math Modeling, College Pk, MD 20742 USA.
[Ide, Kayo] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Ide, Kayo] Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA.
[Farrara, John D.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
RP Li, ZJ (reprint author), Jet Prop Lab, M-S 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM zhijin.li@jpl.nasa.gov
FU Office of Naval Research [N00014-12-1-093, N00014-10-1-0557]
FX The research described in this publication was carried out, in part, the
Jet Propulsion Laboratory (JPL), California Institute of Technology,
under a contract with the National Aeronautics and Space Administration
(NASA). This research was also supported in part by the Office of Naval
Research (N00014-12-1-093) and (N00014-10-1-0557). The authors thank
Prof. Fuqing Zhang and the anonymous reviewers for comments that were
very helpful in improving the manuscript.
NR 24
TC 7
Z9 7
U1 1
U2 11
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 SEP
PY 2015
VL 143
IS 9
BP 3804
EP 3822
DI 10.1175/MWR-D-14-00384.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CQ0UU
UT WOS:000360313800024
ER
PT J
AU Cooper, BL
Thaisen, K
Chang, BC
Lee, TS
McKay, DS
AF Cooper, B. L.
Thaisen, K.
Chang, B. C.
Lee, T. S.
McKay, D. S.
TI Disintegration of Apollo lunar soil
SO NATURE GEOSCIENCE
LA English
DT Letter
C1 [Cooper, B. L.; Chang, B. C.; Lee, T. S.] Hanyang Univ, Int Space Explorat Res Inst, Ansan 426791, Gyeonggi Do, South Korea.
[Thaisen, K.] Grand Valley State Univ, Geol Dept, Allendale, MI 49401 USA.
[McKay, D. S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Cooper, BL (reprint author), Hanyang Univ, Int Space Explorat Res Inst, 2nd Engn Bldg,1271,Sa 3 Dong, Ansan 426791, Gyeonggi Do, South Korea.
EM bcooper108@gmail.com
NR 9
TC 2
Z9 2
U1 4
U2 18
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 SEP
PY 2015
VL 8
IS 9
BP 657
EP 658
PG 2
WC Geosciences, Multidisciplinary
SC Geology
GA CQ1WW
UT WOS:000360392000002
ER
PT J
AU Verstraeten, WW
Neu, JL
Williams, JE
Bowman, KW
Worden, JR
Boersma, KF
AF Verstraeten, Willem W.
Neu, Jessica L.
Williams, Jason E.
Bowman, Kevin W.
Worden, John R.
Boersma, K. Folkert
TI Rapid increases in tropospheric ozone production and export from China
SO NATURE GEOSCIENCE
LA English
DT Article
ID NORTH-AMERICA; TRANSPORT; TRENDS; VARIABILITY; RETRIEVALS; SATELLITE;
BIAS; OMI
AB Rapid population growth and industrialization have driven substantial increases in Asian ozone precursor emissions over the past decade(1), with highly uncertain impacts on regional and global tropospheric ozone levels. According to ozonesonde measurements(2,3), tropospheric ozone concentrations at two Asian sites have increased by 1 to 3% per year since 2000, an increase thought to contribute to positive trends in the ozone levels observed at North America's West Coast(4,5). However, model estimates of the Asian contribution to North American ozone levels are not well-constrained by observations(6,7). Here we interpret Aura satellite measurements of tropospheric concentrations of ozone and its precursor NO2, along with its largest natural source, stratospheric ozone, using the TM5 global chemistry-transport model. We show that tropospheric ozone concentrations over China have increased by about 7% between 2005 and 2010 in response to two factors: a rise in Chinese emissions by about 21% and increased downward transport of stratospheric ozone. Furthermore, we find that transport from China of ozone and its precursors has offset about 43% of the 0.42 DU reduction in free-tropospheric ozone over the western United States that was expected between 2005 and 2010 as a result of emissions reductions associated with federal, state and local air quality policies. We conclude that global efforts may be required to address regional air quality and climate change.
C1 [Verstraeten, Willem W.; Boersma, K. Folkert] Wageningen Univ, Meteorol & Air Qual Grp, NL-6708 PB Wageningen, Netherlands.
[Verstraeten, Willem W.; Williams, Jason E.; Boersma, K. Folkert] Royal Netherlands Meteorol Inst, Satellite Observat, NL-3730 AE De Bilt, Netherlands.
[Neu, Jessica L.; Bowman, Kevin W.; Worden, John R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Verstraeten, WW (reprint author), Wageningen Univ, Meteorol & Air Qual Grp, NL-6708 PB Wageningen, Netherlands.
EM willem.verstraeten@wur.nl
RI Boersma, Klaas/H-4559-2012
OI Boersma, Klaas/0000-0002-4591-7635
FU Netherlands Organization for Scientific Research, NWO Vidi [864.09.001];
NASA ROSES [NNH10ZDA001N-AURA]; European Community's Seventh Framework
Programme [607405 (QA4ECV)]
FX This research was funded by the Netherlands Organization for Scientific
Research, NWO Vidi grant 864.09.001. We acknowledge the free use of
tropospheric NO2 columns from the OMI sensor from
www.temis.nl. 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. A grant
from NASA ROSES NNH10ZDA001N-AURA and from the European Community's
Seventh Framework Programme under grant agreement no 607405 (QA4ECV)
supported part of this research.
NR 33
TC 25
Z9 25
U1 17
U2 73
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 SEP
PY 2015
VL 8
IS 9
BP 690
EP +
DI 10.1038/NGEO2493
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CQ1WW
UT WOS:000360392000012
ER
PT J
AU DiBraccio, GA
Slavin, JA
Imber, SM
Gershman, DJ
Raines, JM
Jackman, CM
Boardsen, SA
Anderson, BJ
Korth, H
Zurbuchen, TH
McNutt, RL
Solomon, SC
AF DiBraccio, Gina A.
Slavin, James A.
Imber, Suzanne M.
Gershman, Daniel J.
Raines, Jim M.
Jackman, Caitriona M.
Boardsen, Scott A.
Anderson, Brian J.
Korth, Haje
Zurbuchen, Thomas H.
McNutt, Ralph L., Jr.
Solomon, Sean C.
TI MESSENGER observations of flux ropes in Mercury's magnetotail
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury's magnetotail; Magnetic reconnection; Magnetic flux ropes;
Magnetospheric physics
ID TRAVELING COMPRESSION REGIONS; INTERPLANETARY MAGNETIC-FIELD; DEEP
GEOMAGNETIC TAIL; ENERGETIC ION BURSTS; ISEE 3 OBSERVATIONS; PLASMA
SHEET; EARTHS MAGNETOTAIL; MAGNETOPAUSE STRUCTURE; 1ST FLYBY;
RECONNECTION
AB We report an investigation of magnetic reconnection in Mercury's magnetotail conducted with MESSENGER Magnetometer and Fast Imaging Plasma Spectrometer measurements during seven "hot seasons" when the periapsis of the spacecraft orbit is on Mercury's dayside. Flux ropes are formed in the cross-tail current sheet by reconnection. We have analyzed 49 flux ropes observed between 1.7 R-M and 2.8 R-M (where R-M is Mercury's radius, or 2440 km) down the tail from the center of the planet, for which minimum variance analysis indicates that the spacecraft passed near the central axis of the structure. An average Alfven speed of 465 km s measured in the plasma sheet surrounding these flux ropes. Under the assumption that the flux ropes moved at the local Alfven speed, the mean duration of 0.74 +/- 0.15 s determined for these structures implies a typical diameter of similar to 345 km, or similar to 0.14 Rm, which is comparable to a proton gyroradius in the plasma sheet of similar to 380 km. We successfully fit the magnetic signatures of 16 flux ropes to a force-free model. The mean radius and core field determined in this manner were similar to 450 km, or similar to 0.18 R-M, and similar to 40 nT, respectively. A superposed epoch analysis of the magnetic field during these events shows variations similar to those observed at Earth, including the presence of a post-plasmoid plasma sheet, filled with disconnected magnetic flux, but the timescales are 40 times shorter at Mercury. The results of this flux rope survey indicate that intense magnetic reconnection occurs frequently in the cross-tail current layer of this small but extremely dynamic magnetosphere. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [DiBraccio, Gina A.; Slavin, James A.; Imber, Suzanne M.; Gershman, Daniel J.; Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Imber, Suzanne M.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Gershman, Daniel J.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
[Jackman, Caitriona M.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Boardsen, Scott A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Boardsen, Scott A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Anderson, Brian J.; Korth, Haje; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
RP DiBraccio, GA (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM gina.a.dibraccio@nasa.gov
RI Slavin, James/H-3170-2012;
OI Slavin, James/0000-0002-9206-724X; Jackman,
Caitriona/0000-0003-0635-7361
FU NASA [NASW-00002, NAS5-97271]; Science and Technology Facilities Council
Ernest Rutherford Fellowship
FX 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.
CMJ is supported by a Science and Technology Facilities Council Ernest
Rutherford Fellowship.
NR 63
TC 11
Z9 11
U1 0
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP
PY 2015
VL 115
SI SI
BP 77
EP 89
DI 10.1016/j.pss.2014.12.016
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ3OP
UT WOS:000360512300011
ER
PT J
AU Cutler, AD
Cantu, LML
Gallo, ECA
Baurle, R
Danehy, PM
Rockwell, R
Goyne, C
McDaniel, J
AF Cutler, Andrew D.
Cantu, Luca M. L.
Gallo, Emanuela C. A.
Baurle, Rob
Danehy, Paul M.
Rockwell, Robert
Goyne, Christopher
McDaniel, Jim
TI Nonequilibrium Supersonic Freestream Studied Using Coherent Anti-Stokes
Raman Spectroscopy
SO AIAA JOURNAL
LA English
DT Article
ID DUAL-MODE SCRAMJET; VIBRATIONAL-RELAXATION; SCATTERING MEASUREMENTS;
CARS MEASUREMENTS; COMBUSTION; PERFORMANCE; FLOW; N2
AB Measurements were conducted at the University of Virginia Supersonic Combustion Facility of the flow in a constant-area duct downstream of a Mach 2 nozzle. The airflow was heated to approximately 1200K in the facility heater upstream of the nozzle. Dual-pump coherent anti-Stokes Raman spectroscopy was used to measure the rotational and vibrational temperatures of N2 and O2 at two planes in the duct. The expectation was that the vibrational temperature would be in equilibrium, because most scramjet facilities are vitiated air facilities and are in vibrational equilibrium. However, with a flow of clean air, the vibrational temperature of N2 along a streamline remains approximately constant between the measurement plane and the facility heater, the vibrational temperature of O2 in the duct is about 1000K, and the rotational temperature is consistent with the isentropic flow. The measurements of N2 vibrational temperature enabled cross-stream nonuniformities in the temperature exiting the facility heater to be documented. The measurements are in agreement with computational fluid dynamics models employing separate lumped vibrational and translational/rotational temperatures. Measurements and computations are also reported for a few percent steam addition to the air. The effect of the steam is to bring the flow to thermal equilibrium, also in agreement with the computational fluid dynamics.
C1 [Cutler, Andrew D.] George Washington Univ, Mech & Aerosp Engn Dept, Newport News, VA 23602 USA.
[Cantu, Luca M. L.; Gallo, Emanuela C. A.] George Washington Univ, Newport News, VA 23602 USA.
[Baurle, Rob] NASA Langley Res Ctr, Hyperson Air Breathing Prop Branch, Hampton, VA 23681 USA.
[Danehy, Paul M.] NASA Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA.
[Rockwell, Robert; Goyne, Christopher; McDaniel, Jim] Univ Virginia, Charlottesville, VA 22904 USA.
RP Cutler, AD (reprint author), George Washington Univ, Mech & Aerosp Engn Dept, 1 Old Oyster Point Rd,Suite 200, Newport News, VA 23602 USA.
FU National Center for Hypersonic Combined Cycle Propulsion [FA
9550-09-1-0611]; NASA Fundamental Aeronautics Program, Hypersonics
Project, Propulsion Discipline
FX The authors would like to thank Roger Reynolds (University of Virginia)
for his support and operation of the wind tunnel. This research was
sponsored by the National Center for Hypersonic Combined Cycle
Propulsion grant FA 9550-09-1-0611. The technical monitors on the grant
are Chiping Li (U.S. Air Force Office of Scientific Research) and Rick
Gaffney (NASA). Support for Paul Danehy was provided by the NASA
Fundamental Aeronautics Program, Hypersonics Project, Propulsion
Discipline.
NR 34
TC 5
Z9 5
U1 1
U2 5
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD SEP
PY 2015
VL 53
IS 9
BP 2762
EP 2770
DI 10.2514/1.J053748
PG 9
WC Engineering, Aerospace
SC Engineering
GA CP6GK
UT WOS:000359983400025
ER
PT J
AU Kathan, W
Hutter, K
Fuller, J
Hautz, J
AF Kathan, Wolfgang
Hutter, Katja
Fueller, Johann
Hautz, Julia
TI Reciprocity vs. Free-Riding in Innovation Contest Communities
SO CREATIVITY AND INNOVATION MANAGEMENT
LA English
DT Article
ID HUMAN COOPERATION; EVOLUTION; COMPETITION; CREATIVITY; ASSISTANCE;
NETWORK; USERS
AB Innovation contest communities are virtual tools for corporations to integrate external knowledge and creativity into the innovation process. Built on both the principle of competition and the advantages of a collaborative community, innovation contest communities constitute special interaction phenomena. The present study explores how different co-operation behaviours, namely reciprocal giving, initial altruistic giving and free-riding, influence the quality of participants' ideas on an open virtual contest platform with more than 2,000 members and more than 4,000 submissions. Our findings show that reciprocity and free-riding are substantial behavioural elements of innovation contest communities leading to different outcomes regarding quality of submitted ideas. With this study, we contribute to a better theoretical understanding of distinctive types of co-operation and free-riding among individuals in the context of open innovation, extending theories of the evolution of co-operation.
C1 [Kathan, Wolfgang; Hutter, Katja; Hautz, Julia] Univ Innsbruck, Sch Management, A-6020 Innsbruck, Austria.
[Fueller, Johann] Univ Innsbruck, Sch Management, Innovat & Entrepreneurship, A-6020 Innsbruck, Austria.
[Fueller, Johann] Harvard Univ, NASA, Tournament Lab, Cambridge, MA 02138 USA.
[Fueller, Johann] HYVE AG, Munich, Germany.
[Fueller, Johann] MIT, Sloan Sch Management, Cambridge, MA 02139 USA.
RP Kathan, W (reprint author), Univ Innsbruck, Sch Management, A-6020 Innsbruck, Austria.
EM wolfgang.kathan@uibk.ac.at; katja.hutter@uibk.ac.at;
johann.fueller@uibk.ac.at; julia.hautz@uibk.ac.at
FU University of Innsbruck
FX We would like to thank Bombardier Transportation for supporting us in
gathering the data for this study. We are also grateful to the vice
rector of research at the University of Innsbruck for the provision of
funding to Wolfgang Kathan ("Doktoratsstipendium aus der
Nachwuchsforderung").
NR 52
TC 0
Z9 0
U1 3
U2 22
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0963-1690
EI 1467-8691
J9 CREAT INNOV MANAG
JI Creat. Innov. Manag.
PD SEP
PY 2015
VL 24
IS 3
BP 537
EP 549
DI 10.1111/caim.12107
PG 13
WC Management
SC Business & Economics
GA CP4QA
UT WOS:000359866100013
ER
PT J
AU Medellin-Azuara, J
MacEwan, D
Howitt, RE
Koruakos, G
Dogrul, EC
Brush, CF
Kadir, TN
Harter, T
Melton, F
Lund, JR
AF Medellin-Azuara, Josu
MacEwan, Duncan
Howitt, Richard E.
Koruakos, George
Dogrul, Emin C.
Brush, Charles F.
Kadir, Tariq N.
Harter, Thomas
Melton, Forrest
Lund, Jay R.
TI Hydro-economic analysis of groundwater pumping for irrigated agriculture
in California's Central Valley, USA
SO HYDROGEOLOGY JOURNAL
LA English
DT Article
DE Agriculture; USA; Hydro-economics; Groundwater management; Remote
sensing; Optimization
ID WATER; BASIN
AB As in many places, groundwater in California (USA) is the major alternative water source for agriculture during drought, so groundwater's availability will drive some inevitable changes in the state's water management. Currently, agricultural, environmental, and urban uses compete for groundwater, resulting in substantial overdraft in dry years with lowering of water tables, which in turn increases pumping costs and reduces groundwater pumping capacity. In this study, SWAP (an economic model of agricultural production and water use in California) and C2VISim (the California Department of Water Resources groundwater model for California's Central Valley) are connected. This paper examines the economic costs of pumping replacement groundwater during drought and the potential loss of pumping capacity as groundwater levels drop. A scenario of three additional drought years continuing from 2014 show lower water tables in California's Central Valley and loss of pumping capacity. Places without access to groundwater and with uncertain surface-water deliveries during drought are the most economically vulnerable in terms of crop revenues, employment and household income. This is particularly true for Tulare Lake Basin, which relies heavily on water imported from the Sacramento-San Joaquin Delta. Remote-sensing estimates of idle agricultural land between 2012 and 2014 confirm this finding. Results also point to the potential of a portfolio approach for agriculture, in which crop mixing and conservation practices have substantial roles.
C1 [Medellin-Azuara, Josu; Howitt, Richard E.; Koruakos, George; Harter, Thomas; Lund, Jay R.] Univ Calif Davis, Davis, CA 95616 USA.
[MacEwan, Duncan; Howitt, Richard E.] ERA Econ, Davis, CA 95616 USA.
[Dogrul, Emin C.; Brush, Charles F.; Kadir, Tariq N.] Calif Dept Water Resources, Sacramento, CA 95814 USA.
[Melton, Forrest] Calif State Univ, Seaside, CA 93955 USA.
[Melton, Forrest] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Medellin-Azuara, J (reprint author), Univ Calif Davis, One Shields Ave, Davis, CA 95616 USA.
EM jmedellin@ucdavis.edu
FU California Department of Food and Agriculture; University of California,
Davis, Office of the Chancellor
FX Authors are thankful for the funding provided by the California
Department of Food and Agriculture and the University of California,
Davis, Office of the Chancellor. SWAP data assembly work from Dr.
Stephen Hatchett (CH2M Hill) and Kabir Tumber (ERA Economics) is
acknowledged. Authors are grateful for the research assistance from
students and staff including Andrew Bell, Alyssa Obester, Nadya
Alexander, Rui Hui, Nicholas Santos and Paula Torres, and project
management from Cathryn Lawrence.
NR 24
TC 6
Z9 6
U1 15
U2 100
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1431-2174
EI 1435-0157
J9 HYDROGEOL J
JI Hydrogeol. J.
PD SEP
PY 2015
VL 23
IS 6
BP 1205
EP 1216
DI 10.1007/s10040-015-1283-9
PG 12
WC Geosciences, Multidisciplinary; Water Resources
SC Geology; Water Resources
GA CP3KD
UT WOS:000359776900012
ER
PT J
AU Cater, CR
Xiao, XR
Goldberg, RK
Kohlman, LW
AF Cater, Christopher R.
Xiao, Xinran
Goldberg, Robert K.
Kohlman, Lee W.
TI Single Ply and Multi-Ply Braided Composite Response Predictions Using
Modified Subcell Approach
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
ID FABRIC-REINFORCED COMPOSITES; LAP SHEAR JOINT; TEXTILE COMPOSITES;
MECHANICAL-PROPERTIES; STIFFNESS PREDICTION; FAILURE ANALYSIS; PART 2;
WOVEN; STRENGTH; MODEL
AB In this work, the modeling of triaxially braided composites was explored through a subcell approach using an improved semianalytical discretization scheme. The unit cell of the braided composite was divided into four unique subcells, each approximated by a mosaic stacking of unidirectional composite plies and modeled through the use of layered-shell elements within the finite- element model. Two subcell discretization schemes were investigated: a model explicitly capturing pure matrix regions, and a model which absorbed pure matrix pockets into neighboring tow plies. Differences in the mesostructure between single- ply and multi- ply braid coupons were addressed through modifications to the subcell discretization. The absorbed matrix model simulated the unique out- of- plane deformations observed experimentally in single- ply tensile tests with acceptable moduli predictions. An investigation of single- shell versus multi- shell coupons for the analysis of multi- ply braids revealed the through- thickness modeling approach was found to have a significant effect on the apparent transverse modulus. Improved moduli predictions in both the axial and transverse directions were obtained by explicitly modeling braided plies with individual layers of shell elements. (C) 2014 American Society of Civil Engineers.
C1 [Cater, Christopher R.; Xiao, Xinran] Michigan State Univ, Composite Vehicle Res Ctr, Mech Engn, Lansing, MI 48910 USA.
[Goldberg, Robert K.; Kohlman, Lee W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Cater, CR (reprint author), Michigan State Univ, Composite Vehicle Res Ctr, Mech Engn, Lansing, MI 48910 USA.
EM caterchr@msu.edu
NR 42
TC 2
Z9 2
U1 2
U2 8
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 SEP
PY 2015
VL 28
IS 5
AR UNSP 04014117
DI 10.1061/(ASCE)AS.1943-5525.0000445
PG 12
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA CP5PP
UT WOS:000359936100002
ER
PT J
AU Tian, ZH
Yu, LY
Leckey, C
AF Tian, Zhenhua
Yu, Lingyu
Leckey, Cara
TI Delamination detection and quantification on laminated composite
structures with Lamb waves and wavenumber analysis
SO JOURNAL OF INTELLIGENT MATERIAL SYSTEMS AND STRUCTURES
LA English
DT Article; Proceedings Paper
CT 24th International Conference on Adaptive Structures and Technologies
(ICAST)
CY OCT 06-09, 2013
CL Aruba, NETH ANTILLES
DE Lamb waves; frequency-wavenumber analysis; elastodynamic finite
integration technique simulation; delamination quantification
ID GUIDED-WAVES; DAMAGE; INTEGRATION; CURVES; IMPACT
AB Laminated composites are susceptible to delamination due to their weak transverse tensile and interlaminar shear strengths as compared to their in-plane properties. Delamination damage can occur internally, where it is not visible to the naked eye. Development of reliable, quantitative techniques for detecting delamination damage in laminated composite components will be imperative for safe and functional optimally designed next-generation composite structures. In this article, we study the potential of using Lamb waves for delamination detection and quantification, using model-assisted data acquisition. Novel wavenumber analysis approaches are developed and discussed to show how they can be used to investigate Lamb wave interactions with delaminated plies. Ultrasonic wave simulations are implemented to provide both in-plane and out-of-plane wave motion for the wavenumber studies. The out-of-plane results are verified against data obtained from experimental tests. It is found that the wavenumber methods can not only determine the delaminated region of the plate and its length, but can also identify the plies between which the delamination occurs. We envision that the wavenumber approaches can lead to a complete delamination quantification in the future.
C1 [Tian, Zhenhua; Yu, Lingyu] Univ S Carolina, Dept Mech Engn, Columbia, SC 29208 USA.
[Leckey, Cara] NASA Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA USA.
RP Yu, LY (reprint author), Univ S Carolina, Dept Mech Engn, 300 Main St, Columbia, SC 29208 USA.
EM yu3@cec.sc.edu
FU University of South Carolina SPARC graduate fellowship; SC NASA EPSCoR
Research and Education Awards Program (REAP) [21-NE-USC_Yu-RGP]
FX The authors would like to acknowledge and thank (1) the
non-reimbursement Space Act Umbrella Agreement SAA1-1181 between South
Carolina Research Foundation (SCRF) and the National Aeronautics and
Space Administration (NASA) Langley Research Center, (2) University of
South Carolina SPARC graduate fellowship, and (3) SC NASA EPSCoR
Research and Education Awards Program (REAP) 21-NE-USC_Yu-RGP.
NR 43
TC 7
Z9 7
U1 0
U2 9
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1045-389X
EI 1530-8138
J9 J INTEL MAT SYST STR
JI J. Intell. Mater. Syst. Struct.
PD SEP
PY 2015
VL 26
IS 13
BP 1723
EP 1738
DI 10.1177/1045389X14557506
PG 16
WC Materials Science, Multidisciplinary
SC Materials Science
GA CP7WP
UT WOS:000360100100013
ER
PT J
AU Devi, VM
Benner, DC
Sung, K
Crawford, TJ
Yu, SS
Brown, LR
Smith, MAH
Mantz, AW
Boudon, V
Ismail, S
AF Devi, V. Malathy
Benner, D. Chris
Sung, Keeyoon
Crawford, Timothy J.
Yu, Shanshan
Brown, Linda R.
Smith, Mary Ann H.
Mantz, Arlan W.
Boudon, Vincent
Ismail, Syed
TI Self- and air-broadened line shapes in the 2 nu(3) P and R branches of
(CH4)-C-12
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Methane; Lorentz width; Pressure-shift; Temperature dependence;
Relaxation matrix elements; Speed dependence
ID OVERLAPPING SPECTRAL-LINES; MULTISPECTRUM ANALYSIS; TEMPERATURE
DEPENDENCES; METHANE LINES; CM(-1) REGION; 2V(3) BAND; MU-M; N-2;
PARAMETERS; CH4
AB In this paper we report line shape parameters of (CH4)-C-12 for several hundred 2 nu(3) transitions in the spectral regions 5891-5996 cm(-1) (P branch) and 6015-6115 cm(-1) (R branch). Air- and self-broadening coefficients were measured as a function of temperature; line mixing via off-diagonal relaxation matrix element coefficients was also obtained for 47 transition pairs. In total, nearly 1517 positions and intensities were retrieved, but many transitions were too weak for the line shape study. For this analysis, we used 25 high-resolution (0.0056 and 0.0067 cm(-1)) and high signal-to-noise (S/N) spectra of high-purity (CH4)-C-12 and the same high-purity (CH4)-C-12 broadened by dry air recorded at different sample temperatures between 130 K and 295 K with the Bruker IFS 125HR Fourier transform spectrometer at JPL. Three different absorption cells were used (1) a White cell set to a path length of 13.09 m for room temperature data, (2) a single-pass 0.2038 m long coolable cell (for self-broadening) and (3) a multipass cell with 20.941 m total path coolable Herriott cell (for air-broadening). In total there were 13 spectra with pure (CH4)-C-12 (0.27-599 Torr) and 12 air-broadened spectra with total sample pressures of 80-805 Torr and volume mixing ratios (VMR) of methane between 0.18 and 1.0. An interactive multispectrum nonlinear least-squares technique was employed to fit the individual P10-P1 and R0-R10 manifolds in all the spectra simultaneously. Results obtained from the present analysis are compared to other recent measurements. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Devi, V. Malathy; Benner, D. Chris] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Sung, Keeyoon; Crawford, Timothy J.; Yu, Shanshan; Brown, Linda R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Smith, Mary Ann H.; Ismail, Syed] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
[Mantz, Arlan W.] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA.
[Boudon, Vincent] Univ Bourgogne Franche Comte, Lab Interdisciplinaire Carnot Bourgogne, CNRS, UMR 6303, F-21078 Dijon, France.
RP Devi, VM (reprint author), Coll William & Mary, Dept Phys, Box 8795, Williamsburg, VA 23187 USA.
EM malathy.d.venkataraman@nasa.gov
RI Yu, Shanshan/D-8733-2016; Sung, Keeyoon/I-6533-2015
FU NASA's Atmospheric Composition Laboratory (ACLAB) program; ANR
[BLAN08-2_321467]
FX The research performed at the College of William and Mary is supported
by NASA's Atmospheric Composition Laboratory (ACLAB) program. Part of
the research conducted at the Jet Propulsion Laboratory (JPL),
California Institute of Technology, Connecticut College and NASA Langley
Research Center is performed under contract with National Aeronautics
and Space Administration. Dr. Boudon acknowledges funding from the ANR
Project "CH4@Titan" (Ref: BLAN08-2_321467). The authors thank H. Tran
for providing the list of predicted off-diagonal relaxation matrix
element coefficients and their temperature dependence exponents.
NR 57
TC 7
Z9 7
U1 0
U2 14
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD SEP
PY 2015
VL 315
SI SI
BP 114
EP 136
DI 10.1016/j.jms.2015.05.003
PG 23
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA CP6WG
UT WOS:000360028300018
ER
PT J
AU Nabity, JA
Lee, JM
AF Nabity, James A.
Lee, Jeffrey M.
TI Low temperature ozone oxidation of solid waste surrogates
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Ozone oxidation; Waste treatment; Solid wastes; Mixed wastes; Plastics;
Sterilization
AB Solid waste management presents a significant challenge to human spaceflight and especially, long-term missions beyond Earth orbit. A six-month mission will generate over 300 kg of solid wastes per crewmember that must be dealt with to eliminate the need for storage and prevent it from becoming a biological hazard to the crew. There are several methods for the treatment of wastes that include oxidation via ozone, incineration, microbial oxidation or pyrolysis and physical methods such as microwave drying and compaction. In recent years, a low temperature oxidation process using ozonated water has been developed for the chemical conversion of organic wastes to CO2 and H2O. Experiments were conducted to evaluate the rate and effectiveness with which ozone oxidized several different waste materials. Increasing the surface area by chopping or shredding the solids into small pieces more than doubled the rate of oxidation. A greater flow of ozone and agitation of the ozonated water system also increased processing rates. Of the materials investigated, plastics have proven the most difficult to oxidize. The processing of plastics above the glass transition temperatures caused the plastics to clump together which reduced the exposed surface area, while processing at lower temperatures reduced surface reaction kinetics. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Nabity, James A.] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
[Lee, Jeffrey M.] NASA, Ames Res Ctr, Bioengn Branch, Moffett Field, CA 95032 USA.
RP Nabity, JA (reprint author), Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA.
EM james.nabity@colorado.edu
FU NASA Ames Research Center [NNA06CA57C]
FX This research was supported in part by Mr. John Fisher of the NASA Ames
Research Center under contract NNA06CA57C. Further, the authors
acknowledge TDA Research, Inc. for providing data from ozone oxidation
experiments with model waste materials and mixed solids waste
surrogates.
NR 22
TC 0
Z9 0
U1 4
U2 8
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD SEP 1
PY 2015
VL 56
IS 5
BP 970
EP 981
DI 10.1016/j.asr.2015.05.026
PG 12
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA CO9NK
UT WOS:000359502300016
ER
PT J
AU Melroy, HR
Wilson, EL
Clarke, GB
Ott, LE
Mao, J
Ramanathan, AK
McLinden, ML
AF Melroy, H. R.
Wilson, E. L.
Clarke, G. B.
Ott, L. E.
Mao, J.
Ramanathan, A. K.
McLinden, M. L.
TI Autonomous field measurements of CO2 in the atmospheric column with the
miniaturized laser heterodyne radiometer (Mini-LHR)
SO APPLIED PHYSICS B-LASERS AND OPTICS
LA English
DT Article
ID CARBON-DIOXIDE; INSTRUMENT; DATABASE; NETWORK; FLUX
AB We present column CO2 measurements taken by the passive miniaturized laser heterodyne radiometer (Mini-LHR) at 1611.51 nm at the Mauna Loa Observatory in Hawaii. The Mini-LHR was operated autonomously, during the month of May 2013 at this site, working in tandem with an AERONET sun photometer that measures aerosol optical depth at 15-min intervals during daylight hours. Laser heterodyne radiometry has been used since the 1970s to measure atmospheric gases such as ozone, water vapor, methane, ammonia, chlorine monoxide, and nitrous oxide. This iteration of the technology utilizes distributed feedback lasers to produce a low-cost, small, portable sensor that has potential for global deployment. Applications of this instrument include supplementation of existing monitoring networks to provide denser global coverage, providing validation for larger satellite missions, and targeting regions of carbon flux uncertainty. Also presented here are preliminary retrieval analysis and the performance analysis that demonstrate that the Mini-LHR responds extremely well to changes in the atmospheric absorption.
C1 [Melroy, H. R.; Clarke, G. B.] Amer Univ, Washington, DC 20016 USA.
[Wilson, E. L.] NASA, Goddard Space Flight Ctr, Laser Remote Sensing Lab, Greenbelt, MD 20771 USA.
[Ott, L. E.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Mao, J.; Ramanathan, A. K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[McLinden, M. L.] NASA, Goddard Space Flight Ctr, Microwave Instrument & Technol Branch, Greenbelt, MD 20771 USA.
RP Melroy, HR (reprint author), Amer Univ, 4400 Massachusetts Ave, Washington, DC 20016 USA.
EM HilaryMelroy@gmail.com
RI Ott, Lesley/E-2250-2012
FU NASA Goddard Space Flight Center
FX We would like to thank John Barnes (NOAA) and Preston Sato (NOAA) at the
Mauna Loa Observatory, and Scotty Malta at Castle Airport. We would also
like to thank Brent Holben (NASA) and the AERONET team, Houston Miller
(The George Washington University), Tom McGee (NASA), Larry Twigg
(SSAI), and Jim Abshire (NASA) for their ongoing collaboration. This
work was supported through NASA Goddard Space Flight Center's Internal
Research and Development (IRAD) and Science Innovation Fund (SIF)
programs.
NR 28
TC 3
Z9 3
U1 3
U2 16
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0946-2171
EI 1432-0649
J9 APPL PHYS B-LASERS O
JI Appl. Phys. B-Lasers Opt.
PD SEP
PY 2015
VL 120
IS 4
BP 609
EP 615
DI 10.1007/s00340-015-6172-3
PG 7
WC Optics; Physics, Applied
SC Optics; Physics
GA CP3WZ
UT WOS:000359814800004
ER
PT J
AU Morrison, CL
Springmann, MJ
Shroades, KM
Stone, RP
AF Morrison, C. L.
Springmann, M. J.
Shroades, K. M.
Stone, R. P.
TI Development of twelve microsatellite loci in the red tree corals Primnoa
resedaeformis and Primnoa pacifica
SO CONSERVATION GENETICS RESOURCES
LA English
DT Article
DE Primnoa; Cold-water coral; Mid-Atlantic Canyons; Gulf of Alaska;
Microsatellites
ID PRIMERS
AB A suite of tetra-, penta-, and hexa-nucleotide microsatellite loci were developed from Roche 454 pyrosequencing data for the cold-water octocorals Primnoa resedaeformis and P. pacifica. Twelve of 98 primer sets tested consistently amplified in 30 P. resedaeformis samples from Baltimore Canyon (western North Atlantic Ocean) and in 24 P. pacifica samples (Shutter Ridge, eastern Gulf of Alaska). The loci displayed moderate levels of allelic diversity (average 7.5 alleles/locus) and heterozygosity (average 47 %). Levels of genetic diversity were sufficient to produce unique multi-locus genotypes and to distinguish species. These common species are long-lived (hundreds of years) and provide essential fish habitat (P. pacifica), yet populations are provided little protection from human activities. These loci will be used to determine regional patterns of population connectivity to inform effective marine spatial planning and ecosystem-based fisheries management.
C1 [Morrison, C. L.; Springmann, M. J.; Shroades, K. M.] US Geol Survey, Leetown Sci Ctr, Kearneysville, WV 25430 USA.
[Stone, R. P.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK USA.
RP Morrison, CL (reprint author), US Geol Survey, Leetown Sci Ctr, 11649 Leetown Rd, Kearneysville, WV 25430 USA.
EM cmorrison@usgs.gov
FU USGS Ecosystems Mission Area, Outer Continental Shelf Program; NOAA's
Deep-sea Coral Research and Technology Program; BOEM
FX Funding was provided by the USGS Ecosystems Mission Area, Outer
Continental Shelf Program, NOAA's Deep-sea Coral Research and Technology
Program, and was sponsored by BOEM. Special thanks to M. Andersen, A.
Demopoulos, C. Kellogg and D.K. Coykendall (USGS), and G. Boland (BOEM).
Any use of trade, product, or firm names is for descriptive purposes
only and does not imply endorsement by the U.S. government.
NR 5
TC 0
Z9 0
U1 3
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1877-7252
EI 1877-7260
J9 CONSERV GENET RESOUR
JI Conserv. Genet. Resour.
PD SEP
PY 2015
VL 7
IS 3
BP 763
EP 765
DI 10.1007/s12686-015-0455-1
PG 3
WC Biodiversity Conservation; Genetics & Heredity
SC Biodiversity & Conservation; Genetics & Heredity
GA CO9UM
UT WOS:000359521500038
ER
PT J
AU Cao, N
Lee, H
Jung, HC
AF Cao, Ning
Lee, Hyongki
Jung, Hahn Chul
TI Mathematical Framework for Phase-Triangulation Algorithms in
Distributed-Scatterer Interferometry
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Differential interferometric synthetic aperture radar (DInSAR);
distributed scatterer (DS) interferometry; persistent scatterer (PS)
interferometry (PSI); phase triangulation (PT); synthetic aperture radar
(SAR)
ID SAR INTERFEROMETRY; STATISTICS
AB To improve the spatial density of measurement points of persistent-scatterer interferometry, distributed scatterer (DS) should be considered and processed. An important procedure in DS interferometry is the phase triangulation (PT). This letter introduces two modified PT algorithms (i.e., equal-weighted PT and coherence-weighted PT) and analyzes the mathematical relations between different published PT methods (i.e., the maximum-likelihood phase estimator, least squares estimator, and eigendecomposition-based phase estimators). The analysis shows that the above five PT methods share very similar mathematical forms with different weight values in the estimation procedure.
C1 [Cao, Ning; Lee, Hyongki] Univ Houston, Dept Civil & Environm Engn, Houston, TX 77204 USA.
[Cao, Ning; Lee, Hyongki] Univ Houston, Natl Ctr Airborne Laser Mapping, Houston, TX 77204 USA.
[Jung, Hahn Chul] NASA, Goddard Space Flight Ctr, Off Appl Sci, Greenbelt, MD 20771 USA.
[Jung, Hahn Chul] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Cao, N (reprint author), Univ Houston, Dept Civil & Environm Engn, Houston, TX 77204 USA.
EM ncao5@uh.edu
OI Cao, Ning/0000-0003-2880-8565
FU National Center for Airborne Laser Mapping via project NSF [EAR-1043051]
FX This work was supported by the National Center for Airborne Laser
Mapping via project NSF EAR-1043051.
NR 18
TC 2
Z9 2
U1 0
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
EI 1558-0571
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD SEP
PY 2015
VL 12
IS 9
BP 1838
EP 1842
DI 10.1109/LGRS.2015.2430752
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 CP0QB
UT WOS:000359579000008
ER
PT J
AU De Lannoy, GJM
Reichle, RH
Peng, JZ
Kerr, Y
Castro, R
Kim, EJ
Liu, Q
AF De Lannoy, Gabrielle J. M.
Reichle, Rolf H.
Peng, Jinzheng
Kerr, Yann
Castro, Rita
Kim, Edward J.
Liu, Qing
TI Converting Between SMOS and SMAP Level-1 Brightness Temperature
Observations Over Nonfrozen Land
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Atmosphere; brightness temperature (Tb); galaxy; soil moisture; Soil
Moisture Active Passive (SMAP); Soil Moisture Ocean Salinity (SMOS)
ID RADIATIVE-TRANSFER MODEL; L-BAND
AB The Soil Moisture and Ocean Salinity (SMOS) and Soil Moisture Active Passive (SMAP) missions provide Level-1 brightness temperature (Tb) observations that are used for global soil moisture estimation. However, the nature of these Tb data differs: the SMOS Tb observations contain atmospheric and select reflected extraterrestrial ("Sky") radiation, whereas the SMAP Tb data are corrected for these contributions, using auxiliary near-surface information. Furthermore, the SMOS Tb observations are multiangular, whereas the SMAP Tb is measured at 40 degrees incidence angle only. This letter discusses how SMOS Tb, SMAP Tb, and radiative transfer modeling components can be aligned in order to enable a seamless exchange of SMOS and SMAP Tb data in soil moisture retrieval and assimilation systems. The aggregated contribution of the atmospheric and reflected Sky radiation is, on average, about 1 K for horizontally polarized Tb and 0.5 K for vertically polarized Tb at 40 degrees incidence angle, but local and short-term values regularly exceed 5 K.
C1 [De Lannoy, Gabrielle J. M.; Reichle, Rolf H.; Peng, Jinzheng; Kim, Edward J.; Liu, Qing] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[De Lannoy, Gabrielle J. M.; Peng, Jinzheng] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Kerr, Yann] Ctr Etud Spatiales Biosphere, F-31401 Toulouse, France.
[Castro, Rita] DEIMOS Engenharia, P-1998023 Lisbon, Portugal.
[Liu, Qing] Sci Syst & Applicat, Lanham, MD 20706 USA.
RP De Lannoy, GJM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM gabrielle.delannoy@nasa.gov
RI Reichle, Rolf/E-1419-2012
FU NASA Soil Moisture Active Passive mission
FX This work was supported by the NASA Soil Moisture Active Passive
mission.
NR 12
TC 2
Z9 2
U1 7
U2 19
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
EI 1558-0571
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD SEP
PY 2015
VL 12
IS 9
BP 1908
EP 1912
DI 10.1109/LGRS.2015.2437612
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 CP0QB
UT WOS:000359579000022
ER
PT J
AU Pedersen, L
Smith, T
Lee, SY
Cabrol, N
AF Pedersen, Liam
Smith, Trey
Lee, Susan Y.
Cabrol, Nathalie
TI Planetary LakeLander-A Robotic Sentinel to Monitor Remote Lakes
SO JOURNAL OF FIELD ROBOTICS
LA English
DT Article
AB This field report describes the design and operations of the Planetary LakeLander (PLL) probe and its ground data systems. LakeLander's primary mission is to characterize the physical, chemical, and biological processes occurring in a high-altitude lake, and how they are being impacted by rapid deglaciation. LakeLander's secondary purpose is to test operation concepts for future exploration of Titan's lakes. The LakeLander probe is a permanently anchored buoy that measures both surface meteorology and water quality parameters in the top 40m of the water column. The concept of operations calls for the probe to continue collecting and downlinking data through the Andean winter, when the lake is inaccessible; this drives the power system design and forces a strong focus on system reliability, analogous to a space mission. The PLL ground data system provides the central archive of downlinked data. They are structured around a unified data-sharing web site that includes tools for mapping, data visualization, documentation, and numerical analysis. The web site provides a hub for engaging the science team and enables interdisciplinary collaboration. This report concludes with lessons learned during field deployment and several months of remote operations on the lake. Among the conclusions: (1) the choice to use an off-the-shelf profiling system has proven wise; (2) effective maintenance of a long-lived remote system requires extensive measurement, logging, and display of as many system variables as possible; and (3) the visualization sandbox component of the data-sharing web site has made numerical analysis of probe data much easier and more accessible to the entire interdisciplinary science team.
C1 [Pedersen, Liam; Smith, Trey] NASA, Ames Res Ctr, Carnegie Mellon Univ, Moffett Field, CA 94035 USA.
[Lee, Susan Y.] NASA, Ames Res Ctr, Stinger Ghaffarian Technol, Moffett Field, CA 94035 USA.
[Cabrol, Nathalie] NASA, Ames Res Ctr, Div Space Sci, Carl Sagan Ctr,SETI Inst, Mountain View, CA 94035 USA.
RP Pedersen, L (reprint author), NASA, Ames Res Ctr, Carnegie Mellon Univ, Moffett Field, CA 94035 USA.
EM Liam.Pedersen@nasa.gov; Trey.Smith@nasa.gov; Susan.Y.Lee@nasa.gov;
Nathalie.A.Cabrol@nasa.gov
FU NASA's Astrobiology Science and Technology for Exploring Planets (ASTEP)
program
FX This work is funded by NASA's Astrobiology Science and Technology for
Exploring Planets (ASTEP) program. Additional expertise was drawn from
the Intelligent Robotics Group at NASA's Ames Research Center,
specifically Mark Micire, Matt Deans, David Lees, Tamar Cohen, and Vinh
To.
NR 16
TC 0
Z9 0
U1 1
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1556-4959
EI 1556-4967
J9 J FIELD ROBOT
JI J. Field Robot.
PD SEP
PY 2015
VL 32
IS 6
BP 860
EP 879
DI 10.1002/rob.21545
PG 20
WC Robotics
SC Robotics
GA CP1AF
UT WOS:000359607500002
ER
PT J
AU Tweddle, BE
Saenz-Otero, A
Leonard, JJ
Miller, DW
AF Tweddle, Brent E.
Saenz-Otero, Alvar
Leonard, John J.
Miller, David W.
TI Factor Graph Modeling of Rigid-body Dynamics for Localization, Mapping,
and Parameter Estimation of a Spinning Object in Space
SO JOURNAL OF FIELD ROBOTICS
LA English
DT Article
ID ATTITUDE ESTIMATION; CONSTRAINT; ALIGNMENT
AB This paper presents a new approach for solving the simultaneous localization and mapping problem for inspecting an unknown and uncooperative object that is spinning about an arbitrary axis in space. This approach probabilistically models the six degree-of-freedom rigid-body dynamics in a factor graph formulation. Using the incremental smoothing and mapping system, this method estimates a feature-based map of the target object, as well as this object's position, orientation, linear velocity, angular velocity, center of mass, principal axes, and ratios of inertia. This solves an important problem for spacecraft proximity operations. Additionally, it provides a generic framework for incorporating rigid-body dynamics that may be applied to a number of other terrestrial-based applications. To evaluate this approach, the Synchronized Position Hold Engage Reorient Experimental Satellites (SPHERES) were used as a testbed within the microgravity environment of the International Space Station. The SPHERES satellites, using body-mounted stereo cameras, captured a dataset of a target object that was spinning at ten rotations per minute about its unstable, intermediate axis. This dataset was used to experimentally evaluate the approach described in this paper, and it showed that it was able to estimate a geometric map and the position, orientation, linear and angular velocities, center of mass, and ratios of inertia of the target object.
C1 [Tweddle, Brent E.; Saenz-Otero, Alvar; Miller, David W.] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA.
[Leonard, John J.] MIT, Dept Mech Engn, Cambridge, MA 02139 USA.
RP Tweddle, BE (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM tweddle@jpl.nasa.gov; alvarso@mit.edu; jleonard@mit.edu; millerd@mit.edu
FU DARPA; NASA; Air Force Space Test Program; NASA Ames; Defense Advanced
Research Project Agency's Integrated Research Experiments (InSPIRE)
program [NNH11CC25C]
FX Brent Tweddle would like to thank the members of his doctoral committee,
Prof. David W. Miller, Dr. Alvar Saenz-Otero, Prof. John J. Leonard, and
Dr. Larry H. Matthies, as well as the readers of his doctoral thesis,
Dr. Glen Henshaw, Prof. John Deyst, Prof. Emilio Frazzoli, Prof.
Nicholas Roy, and Prof. Sheila Widnall. The authors would also like to
thank DARPA and NASA for their funding and support of this research, and
the SPHERES VERTIGO team at MIT and Aurora Flight Sciences for their
work on the Goggles, including our support from the Air Force Space Test
Program and NASA Ames. This research was funded by the Defense Advanced
Research Project Agency's Integrated Research Experiments (InSPIRE)
program under contract NNH11CC25C.
NR 51
TC 1
Z9 1
U1 2
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1556-4959
EI 1556-4967
J9 J FIELD ROBOT
JI J. Field Robot.
PD SEP
PY 2015
VL 32
IS 6
BP 897
EP 933
DI 10.1002/rob.21548
PG 37
WC Robotics
SC Robotics
GA CP1AF
UT WOS:000359607500004
ER
PT J
AU Thomas, BF
Famiglietti, JS
AF Thomas, Brian F.
Famiglietti, James S.
TI Sustainable Groundwater Management in the Arid Southwestern US:
Coachella Valley, California
SO WATER RESOURCES MANAGEMENT
LA English
DT Article
DE Sustainable groundwater management; Groundwater trends; Statistical
analysis; California groundwater
ID WATER-BUDGET MYTH; AQUIFER SYSTEM; COLORADO RIVER; TREND ANALYSIS;
UNITED-STATES; SAFE YIELD; DROUGHT; STREAMFLOW; FLOW; RESOURCES
AB Sustainable groundwater management requires approaches to assess the influence of climate and management actions on the evolution of groundwater systems. Traditional approaches that apply continuity to assess groundwater sustainability fail to capture the spatial variability of aquifer responses. To address this gap, our study evaluates groundwater elevation data from the Coachella Valley, California, within a groundwater sustainability framework given the adoption of integrative management strategies in the valley. Our study details an innovative approach employing traditional statistical methods to improve understanding of aquifer responses. In this analysis, we evaluate trends at individual groundwater observation wells and regional groundwater behaviors using field significance. Regional elevation trends identified no significant trends during periods of intense groundwater replenishment, active since 1973, despite spatial variability in individual well trends. Our results illustrate the spatially limited effects of groundwater replenishment occur against a setting of long-term groundwater depletion, raising concerns over the definition of sustainable groundwater management in aquifer systems employing integrative management strategies.
C1 [Thomas, Brian F.; Famiglietti, James S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Famiglietti, James S.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Famiglietti, James S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA 92697 USA.
RP Thomas, BF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Brian.F.Thomas@jpl.nasa.gov
FU University of California Office of the President Multicampus Research
and Programs Initiative
FX The authors would like to thank Ian James of the Desert Sun for alerting
us about the growing concern over groundwater overdraft in the valley
and the Coachella Valley Water District and the Desert Water Agency for
supplying groundwater elevation data used in this study. Project support
was provided by the University of California Office of the President
Multicampus Research and Programs Initiative. The research was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration. We wish to thank two anonymous reviewers and
Editor-in-Chief Tsakiris for comments that improved our manuscript.
NR 69
TC 7
Z9 7
U1 17
U2 72
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0920-4741
EI 1573-1650
J9 WATER RESOUR MANAG
JI Water Resour. Manag.
PD SEP
PY 2015
VL 29
IS 12
BP 4411
EP 4426
DI 10.1007/s11269-015-1067-y
PG 16
WC Engineering, Civil; Water Resources
SC Engineering; Water Resources
GA CO8KJ
UT WOS:000359417500012
ER
PT J
AU Gao, F
Hilker, T
Zhu, XL
Anderson, MC
Masek, JG
Wang, PJ
Yang, Y
AF Gao, Feng
Hilker, Thomas
Zhu, Xiaolin
Anderson, Martha C.
Masek, Jeffrey G.
Wang, Peijuan
Yang, Yun
TI Fusing Landsat and MODIS Data for Vegetation Monitoring
SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE
LA English
DT Article
ID SURFACE REFLECTANCE; FOREST; RESOLUTION; MODEL; EVAPOTRANSPIRATION;
DISTURBANCE; PRODUCTS; SCIENCE; IMAGERY
AB Crop condition and natural vegetation monitoring require high resolution remote sensing imagery in both time and space - a requirement that cannot currently be satisfied by any single Earth observing sensor in isolation. The suite of available remote sensing instruments varies widely in terms of sensor characteristics, spatial resolution and acquisition frequency. For example, the Moderate-resolution Imaging Spectroradiometer (MODIS) provides daily global observations at 250m to 1km spatial resolution. While imagery from coarse resolution sensors such as MODIS are typically superior to finer resolution data in terms of their revisit frequency, they lack spatial detail to capture surface features for many applications. The Landsat satellite series provides medium spatial resolution (30m) imagery which is well suited to capturing surface details, but a long revisit cycle (16-day) has limited its use in describing daily surface changes. Data fusion approaches provide an alternative way to utilize observations from multiple sensors so that the fused results can provide higher value than can an individual sensor alone. In this paper, we review the Spatial and Temporal Adaptive Reflectance Fusion Model (STARFM) and two extended data fusion models (STAARCH and ESTARFM) that have been used to fuse MODIS and Landsat data. The fused MODISLandsat results inherit the spatial details of Landsat (30 m) and the temporal revisit frequency of MODIS (daily). The theoretical basis of the fusion approach is described and recent applications are presented. While these approaches can produce imagery with high spatiotemporal resolution, they still rely on the availability of actual satellite images and the quality of ingested remote sensing products. As a result, data fusion is useful for bridging gaps between medium resolution image acquisitions, but cannot replace actual satellite missions.
C1 [Gao, Feng; Anderson, Martha C.; Yang, Yun] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Hilker, Thomas] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA.
[Zhu, Xiaolin] Colorado State Univ, Dept Ecosyst Sci & Sustainabil, Ft Collins, CO 80523 USA.
[Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Wang, Peijuan] Chinese Acad Meteorol Sci, Inst Ecoenvironm & Agrometeorol, Beijing 100081, Peoples R China.
RP Gao, F (reprint author), USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
EM feng.gao@ars.usda.gov; Thomas.Hilker@oregonstate.edu;
zhuxiaolin55@gmail.com; martha.anderson@ars.usda.gov;
jeffrey.g.masek@nasa.gov; wangpj@cams.cma.gov.cn; yun.yang@ars.usda.gov
RI Anderson, Martha/C-1720-2015; Zhu, Xiaolin/K-8175-2012
OI Anderson, Martha/0000-0003-0748-5525; Zhu, Xiaolin/0000-0001-6967-786X
NR 39
TC 8
Z9 8
U1 3
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2168-6831
J9 IEEE GEOSC REM SEN M
JI IEEE Geosci. Remote Sens. Mag.
PD SEP
PY 2015
VL 3
IS 3
BP 47
EP 60
DI 10.1109/MGRS.2015.2434351
PG 14
WC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
SC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
GA EF0GQ
UT WOS:000390004300006
ER
PT J
AU Stauffer, RM
Thompson, AM
Martins, DK
Clark, RD
Goldberg, DL
Loughner, CP
Delgado, R
Dickerson, RR
Stehr, JW
Tzortziou, MA
AF Stauffer, Ryan M.
Thompson, Anne M.
Martins, Douglas K.
Clark, Richard D.
Goldberg, Daniel L.
Loughner, Christopher P.
Delgado, Ruben
Dickerson, Russell R.
Stehr, Jeffrey W.
Tzortziou, Maria A.
TI Bay breeze influence on surface ozone at Edgewood, MD during July 2011
SO JOURNAL OF ATMOSPHERIC CHEMISTRY
LA English
DT Article
DE Ozone; Bay Breeze; Pollution; Edgewood; Mid-Atlantic; DISCOVER-AQ
ID INTERNAL BOUNDARY-LAYERS; POLLUTANT TRANSPORT; HOUSTON; IMPACT;
CLIMATOLOGY; TEMPERATURE; EPISODE; COMPLEX; DEPTH; URBAN
AB Surface ozone (O-3) was analyzed to investigate the role of the bay breeze on air quality at two locations in Edgewood, Maryland (lat: 39.4A degrees, lon: -76.3A degrees) for the month of July 2011. Measurements were taken as part of the first year of NASA's "Deriving Information on Surface Conditions from Column and Vertically Resolved Observations Relevant to Air Quality" (DISCOVER-AQ) Earth Venture campaign and as part of NASA's Geostationary for Coastal and Air Pollution Events Chesapeake Bay Oceanographic campaign with DISCOVER-AQ (Geo-CAPE CBODAQ). Geo-CAPE CBODAQ complements DISCOVER-AQ by providing ship-based observations over the Chesapeake Bay. A major goal of DISCOVER-AQ is determining the relative roles of sources, photochemistry and local meteorology during air quality events in the Mid-Atlantic region of the U.S. Surface characteristics, transport and vertical structures of O-3 during bay breezes were identified using in-situ surface, balloon and aircraft data, along with remote sensing equipment. Localized late day peaks in O-3 were observed during bay breeze days, maximizing an average of 3 h later compared to days without bay breezes. Of the 10 days of July 2011 that violated the U.S. Environmental Protection Agency (EPA) 8 h O-3 standard of 75 parts per billion by volume (ppbv) at Edgewood, eight exhibited evidence of a bay breeze circulation. The results indicate that while bay breezes and the processes associated with them are not necessary to cause exceedances in this area, bay breezes exacerbate poor air quality that sustains into the late evening hours at Edgewood. The vertical and horizontal distributions of O-3 from the coastal Edgewood area to the bay also show large gradients that are often determined by boundary layer stability. Thus, developing air quality models that can sufficiently resolve these dynamics and associated chemistry, along with more consistent monitoring of O-3 and meteorology on and along the complex coastline of Chesapeake Bay must be a high priority.
C1 [Stauffer, Ryan M.; Thompson, Anne M.; Martins, Douglas K.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Clark, Richard D.] Millersville Univ Pennsylvania, Dept Earth Sci, Millersville, PA 17551 USA.
[Goldberg, Daniel L.; Dickerson, Russell R.; Stehr, Jeffrey W.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Loughner, Christopher P.; Tzortziou, Maria A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Loughner, Christopher P.; Tzortziou, Maria A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Delgado, Ruben] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
RP Stauffer, RM (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA.
EM rms5539@psu.edu
RI Dickerson, Russell/F-2857-2010; Delgado, Ruben/F-9753-2016; Thompson,
Anne /C-3649-2014;
OI Dickerson, Russell/0000-0003-0206-3083; Delgado,
Ruben/0000-0002-7133-2462; Stauffer, Ryan/0000-0002-8583-7795; Thompson,
Anne /0000-0002-7829-0920; Loughner, Christopher/0000-0002-3833-2014
FU NASA DISCOVER-AQ grant [NNX10AR39G]; NASA [NNX08AJ15G]
FX Funding and research for this project was provided by the NASA
DISCOVER-AQ grant NNX10AR39G as well as NASA grant NNX08AJ15G. The
authors would like to thank James Crawford, Mary Kleb, Kenneth
Pickering, Gao Chen and all the DISCOVER-AQ participants for their
support and contributions. Thanks also to Lacey Brent for ship and
aircraft measurements with additional support from MDE, and NIST for
calibration assistance. Thanks to Andrew Weinheimer (NCAR), Edwin Gluth,
Laura Warren, Jennifer Hains, Mike Woodman and Dave Krask (MDE), and
Hannah Halliday, Greg Garner, Andra Reed, Debra Kollonige (PSU) for
their assistance and Bill Ryan (PSU) for his early insights into the
potential for bay breeze effects on ozone.
NR 45
TC 17
Z9 17
U1 1
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-7764
EI 1573-0662
J9 J ATMOS CHEM
JI J. Atmos. Chem.
PD SEP
PY 2015
VL 72
IS 3-4
SI SI
BP 335
EP 353
DI 10.1007/s10874-012-9241-6
PG 19
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CX6CP
UT WOS:000365789100008
ER
PT J
AU Ruzicka, A
Grossman, J
Bouvier, A
Herd, CDK
Agee, CB
AF Ruzicka, Alex
Grossman, Jeffrey
Bouvier, Audrey
Herd, Christopher D. K.
Agee, Carl B.
TI The Meteoritical Bulletin, No. 101
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Editorial Material
AB Meteoritical Bulletin 101 contains 2639 meteorites accepted by the Nomenclature Committee in 2012, including 1 fall (Battle Mountain), with 2308 ordinary chondrites, 156 carbonaceous chondrites, 63 HED achondrites, 17 relict meteorites, 16 Rumuruti chondrites, 15 enstatite chondrites, 15 ureilites, 10 iron meteorites, 9 lunar meteorites, 9 primitive achondrites, 8 ungrouped achondrites, 7 mesosiderites, 4 Martian meteorites, and 2 Pallasites, and with 1812 from Antarctica, 437 from Asia, 301 from Africa, 43 from South America, 21 from Europe (including Russia), 21 from North America, 3 from Oceania, and 1 from unknown. Information about approved meteorites can be obtained from the Meteoritical Bulletin Database (MBD) available on line at http://www.lpi.usra.edu/meteor/.
C1 [Ruzicka, Alex] Portland State Univ, Cascadia Meteorite Lab, Dept Geol, Portland, OR 97207 USA.
[Grossman, Jeffrey] NASA Headquarters, Washington, DC 20546 USA.
[Bouvier, Audrey] Western Univ, Dept Earth Sci, London, ON N6A B57, Canada.
[Herd, Christopher D. K.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada.
[Agee, Carl B.] Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
RP Ruzicka, A (reprint author), Portland State Univ, Cascadia Meteorite Lab, Dept Geol, Portland, OR 97207 USA.
EM ruzickaa@pdx.edu
NR 0
TC 1
Z9 1
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2015
VL 50
IS 9
BP 1661
EP 1661
DI 10.1111/maps.12490
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CQ7DE
UT WOS:000360762300011
ER
PT J
AU Ruzicka, A
Grossman, J
Bouvier, A
Herd, CDK
Agee, EB
AF Ruzicka, Alex
Grossman, Jeffrey
Bouvier, Audrey
Herd, Christopher D. K.
Agee, Carl B.
TI The Meteoritical Bulletin, No. 102
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Editorial Material
AB Meteoritical Bulletin 102 contains 3141 meteorites including 12 falls (Boumdeid (2003), Boumdeid (2011), Braunschweig, Chelyabinsk, Dongyang, Draveil, Heyetang, Indian Butte, Katol, Ladkee, Ouadangou, Xining), with 2611 ordinary chondrites, 264 HED achondrites, 124 carbonaceous chondrites, 30 ureilites, 20 Martian meteorites, 16 primitive achondrites, 16 Rumuruti chondrites, 15 mesosiderites, 12 iron meteorites, 10 lunar meteorites, 9 enstatite chondrites, 4 enstatite achondrites, 4 Pallasites, 4 ungrouped achondrites, and 2 angrites, and with 1708 from Antarctica, 956 from Africa, 294 from South America, 126 from Asia, 47 from North America, 6 from Europe (including Russia), and 4 from Oceania. Information about approved meteorites can be obtained from the Meteoritical Bulletin Database (MBD) available on line at http://www.lpi.usra.edu/meteor/.
C1 Portland State Univ, Cascadia Meteorite Lab, Dept Geol, Portland, OR 97207 USA.
NASA Headquarters, Washington, DC 20546 USA.
Western Univ, Dept Earth Sci, London, ON N6A B57, Canada.
Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada.
Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
RP Ruzicka, A (reprint author), Portland State Univ, Cascadia Meteorite Lab, Dept Geol, Portland, OR 97207 USA.
EM ruzickaa@pdx.edu
NR 0
TC 7
Z9 7
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD SEP
PY 2015
VL 50
IS 9
BP 1662
EP 1662
DI 10.1111/maps.12491
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CQ7DE
UT WOS:000360762300012
ER
PT J
AU Gudmundsson, V
Schulze, C
Ganesan, D
Lindvall, M
Wiegand, R
AF Gudmundsson, Vignir
Schulze, Christoph
Ganesan, Dharmalingam
Lindvall, Mikael
Wiegand, Robert
TI Model-based testing of NASA's GMSEC, a reusable framework for ground
system software
SO INNOVATIONS IN SYSTEMS AND SOFTWARE ENGINEERING
LA English
DT Article
DE Middleware; Wrapper; Software bus; Automated test case generation;
Model-based testing; Finite-state machines; Extended finite-state
machines
AB We present an empirical study in which model-based testing (MBT) was applied to the software bus of NASA's Goddard Mission Service Evolution Center (GMSEC), a reusable software framework. The goal was to study the feasibility of using MBT on a real-world software system that was designed to be flexible. GMSEC has three levels of flexibility: 1) loose application coupling through a software bus based on the publish-subscribe architectural style, 2) language independence by providing APIs to the bus in several programming languages, 3) middleware independence by providing wrappers for several middlewares that are supported by the software bus. The novelty brought forward in this paper is that one model and one set of generated test cases were used as the basis to test the software bus for behavioral consistency across multiple programming languages and middleware wrappers. The comparison of costs and benefits from using finite state machines (FSM) vs. extended FSMs (EFSM) when used for MBT on a real-world system is also novel. The case study shows that it was feasible, even for a programmer who neither knew MBT nor the system under test, to successfully apply MBT to a flexible system such as GMSEC and that MBT could within reasonable effort detect non-trivial defects in a fielded system.
C1 [Gudmundsson, Vignir] Reykjavik Univ, Reykjavik, Iceland.
[Schulze, Christoph; Ganesan, Dharmalingam; Lindvall, Mikael] Fraunhofer CESE, College Pk, MD USA.
[Wiegand, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Gudmundsson, V (reprint author), Reykjavik Univ, Reykjavik, Iceland.
EM vignir09@ru.is; cschulze@fc-md.umd.edu; dganesan@fc-md.umd.edu;
mlindvall@fc-md.umd.edu; robert.e.wiegand@nasa.gov
NR 27
TC 1
Z9 1
U1 0
U2 1
PU SPRINGER LONDON LTD
PI LONDON
PA 236 GRAYS INN RD, 6TH FLOOR, LONDON WC1X 8HL, ENGLAND
SN 1614-5046
EI 1614-5054
J9 INNOV SYST SOFTW ENG
JI Innov. Syst. Softw. Eng.
PD SEP
PY 2015
VL 11
IS 3
SI SI
BP 217
EP 232
DI 10.1007/s11334-015-0254-6
PG 16
WC Computer Science, Software Engineering
SC Computer Science
GA CP2QV
UT WOS:000359723000008
ER
PT J
AU Roa, J
Pelaez, J
AF Roa, Javier
Pelaez, Jesus
TI Orbit propagation in Minkowskian geometry
SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY
LA English
DT Article
DE Hyperbolic orbits; Minkowskian geometry; Numerical methods; Comets;
Dromo
ID LONG-PERIOD COMETS; PERTURBED KEPLERIAN MOTIONS; OUTER SOLAR-SYSTEM;
OORT CLOUD; CROSSING ASTEROIDS; RESONANT ASTEROIDS; IDEAL FRAMES; EARTH;
DYNAMICS; REGULARIZATION
AB The geometry of hyperbolic orbits suggests that Minkowskian geometry, and not Euclidean, may provide the most adequate description of the motion. This idea is explored in order to derive a new regularized formulation for propagating arbitrarily perturbed hyperbolic orbits. The mathematical foundations underlying Minkowski space-time are exploited to describe hyperbolic orbits. Hypercomplex numbers are introduced to define the rotations, vectors, and metrics in the problem: the evolution of the eccentricity vector is described on the Minkowski plane in terms of hyperbolic numbers, and the orbital plane is described on the inertial reference using quaternions. A set of eight orbital elements is introduced, namely a time-element, the components of the eccentricity vector in , the semimajor axis, and the components of the quaternion defining the orbital plane. The resulting formulation provides a deep insight into the geometry of hyperbolic orbits. The performance of the formulation in long-term propagations is studied. The orbits of four hyperbolic comets are integrated and the accuracy of the solution is compared to other regularized formulations. The resulting formulation improves the stability of the integration process and it is not affected by the perihelion passage. It provides a level of accuracy that may not be reached by the compared formulations, at the cost of increasing the computational time.
C1 [Roa, Javier; Pelaez, Jesus] Tech Univ Madrid UPM, ETSI Aeronaut, Madrid 28040, Spain.
RP Roa, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM javier.roa@upm.es; j.pelaez@upm.es
OI Roa, Javier/0000-0002-0810-1549
FU Spanish Ministry of Economy and Competitiveness [ESP2013-41634-P];
Spanish Government; La Caixa
FX This work is part of the research Project entitled "Dynamical Analysis,
Advanced Orbit Propagation and Simulation of Complex Space Systems"
(ESP2013-41634-P) supported by the Spanish Ministry of Economy and
Competitiveness. Authors thank Spanish Government for its support. J.
Roa especially thanks "La Caixa" for his doctoral fellowship, H.
Urrutxua for his help with the numerical integration, and D. Amato for
reporting some typos. An anonymous reviewer greatly assisted the authors
in improving this manuscript.
NR 61
TC 5
Z9 5
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0923-2958
EI 1572-9478
J9 CELEST MECH DYN ASTR
JI Celest. Mech. Dyn. Astron.
PD SEP
PY 2015
VL 123
IS 1
BP 13
EP 43
DI 10.1007/s10569-015-9627-2
PG 31
WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications
SC Astronomy & Astrophysics; Mathematics
GA CO4WH
UT WOS:000359161100002
ER
PT J
AU Petropoulos, GP
Ireland, G
Srivastava, PK
AF Petropoulos, George P.
Ireland, Gareth
Srivastava, Prashant K.
TI Evaluation of the Soil Moisture Operational Estimates From SMOS in
Europe: Results Over Diverse Ecosystems
SO IEEE SENSORS JOURNAL
LA English
DT Article
DE CarboEurope; MIRAS; remote sensing; soil moisture; SMOS
ID IN-SITU OBSERVATIONS; LAND-SURFACE MODEL; ENERGY FLUXES; RETRIEVAL;
VALIDATION; SATELLITE; CATCHMENT; ALGORITHM; FOREST; VARIABILITY
AB This study presents the results of an extensive validation of the Soil Moisture and Ocean Salinity mission (SMOS) soil moisture operational product from selected European sites representative of a variety of climatic, environmental, biome, and seasonal conditions. SMOS soil moisture estimates were compared against corresponding in-situ measurements from the CarboEurope observational network. The agreement between the two datasets was evaluated on the basis of a series of statistical metrics. In addition, the effect of variability of site characteristics such as land cover, seasonality, and also that of the Radio Frequency Interference (RFI) effect on SMOS was explored. In overall, the SMOS soil moisture product estimates agreed reasonably well with near concurrent CarboEurope in-situ measurements acquired from the 0-5 cm soil moisture layer. Significant changes in the SMOS performance were observed with local adjustments, such as land cover and seasonal changes. Agreement was found to be higher over low vegetation cover and during the autumn season. The RFI contaminated pixels were filtered out from the pooled datasets, as well as from the seasonally discriminated datasets, which resulted in noticeably improved performances. This paper provides strong supportive evidence of the potential value of the SMOS soil moisture product for hydrometeorological and related studies.
C1 [Petropoulos, George P.; Ireland, Gareth] Dept Geog & Earth Sci, Aberystwyth SY23 3BD, Dyfed, Wales.
[Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Srivastava, Prashant K.] Banaras Hindu Univ, Inst Environm & Sustainable Dev, Varanasi 221005, Uttar Pradesh, India.
RP Petropoulos, GP (reprint author), Dept Geog & Earth Sci, Aberystwyth SY23 3BD, Dyfed, Wales.
EM gep9@aber.ac.uk; gai2@aber.ac.uk; prashant.k.srivastava@nasa.gov
RI Petropoulos, George/F-2384-2013
OI Petropoulos, George/0000-0003-1442-1423
FU European Space Agency (ESA) Support to Science Element (STSE)
[STSE-TEBM-EOPG-TN-08-0005]
FX The preparation of this work was partially supported by the European
Space Agency (ESA) Support to Science Element (STSE) under contract
STSE-TEBM-EOPG-TN-08-0005. George Petropoulos gratefully acknowledges
the financial support provided by the Agency. The views expressed here
are those of the authors solely and do not constitute a statement of
policy, decision, or position on behalf of the NASA or authors'
affiliated institutions.
NR 53
TC 2
Z9 2
U1 3
U2 15
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1530-437X
EI 1558-1748
J9 IEEE SENS J
JI IEEE Sens. J.
PD SEP
PY 2015
VL 15
IS 9
BP 5243
EP 5251
DI 10.1109/JSEN.2015.2427657
PG 9
WC Engineering, Electrical & Electronic; Instruments & Instrumentation;
Physics, Applied
SC Engineering; Instruments & Instrumentation; Physics
GA CN7XI
UT WOS:000358648200065
ER
PT J
AU Bednarcyk, BA
Aboudi, J
Arnold, SM
AF Bednarcyk, Brett A.
Aboudi, Jacob
Arnold, Steven M.
TI Analysis of fiber clustering in composite materials using high-fidelity
multiscale micromechanics
SO INTERNATIONAL JOURNAL OF SOLIDS AND STRUCTURES
LA English
DT Article
DE Composites; Fiber clustering; Modeling; Multiscale; Nonlinearity; Yield
and damage envelopes; High-Fidelity Generalized Method of Cells
ID CERAMIC-MATRIX COMPOSITES; REINFORCED COMPOSITES; PROGRESSIVE DAMAGE;
MICROSTRUCTURE; CELLS
AB A new multiscale micromechanical approach is developed for the prediction of the behavior of fiber reinforced composites in presence of fiber clustering. The developed method is based on a coupled two-scale implementation of the High-Fidelity Generalized Method of Cells theory, wherein both the local and global scales are represented using this micromechanical method. Concentration tensors and effective constitutive equations are established on both scales and linked to establish the required coupling, thus providing the local fields throughout the composite as well as the global properties and effective nonlinear response. Two non-dimensional parameters, in conjunction with actual composite micrographs, are used to characterize the clustering of fibers in the composite. Based on the predicted local fields, initial yield and damage envelopes are generated for various clustering parameters for a polymer matrix composite with both carbon and glass fibers. Nonlinear epoxy matrix behavior is also considered, with results in the form of effective nonlinear response curves, with varying fiber clustering and for two sets of nonlinear matrix parameters. Published by Elsevier Ltd.
C1 [Bednarcyk, Brett A.; Arnold, Steven M.] NASA, Glenn Res Ctr, Cleveland, OH 44256 USA.
[Aboudi, Jacob] Tel Aviv Univ, IL-69978 Tel Aviv, Israel.
RP Bednarcyk, BA (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44256 USA.
EM Brett.A.Bednarcyk@nasa.gov
NR 35
TC 1
Z9 1
U1 3
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0020-7683
EI 1879-2146
J9 INT J SOLIDS STRUCT
JI Int. J. Solids Struct.
PD SEP
PY 2015
VL 69-70
BP 311
EP 327
DI 10.1016/j.ijsolstr.2015.05.019
PG 17
WC Mechanics
SC Mechanics
GA CO5AM
UT WOS:000359172000025
ER
PT J
AU Lee, JN
Cahalan, RF
Wu, DL
AF Lee, Jae N.
Cahalan, Robert F.
Wu, Dong L.
TI The 27-day rotational variations in total solar irradiance observations:
From SORCE/TIM, ACRIMSAT/ACRIM III, and SOHO/VIRGO
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
ID EMPIRICAL MODE DECOMPOSITION; ACTIVE CAVITY RADIOMETER; ULTRAVIOLET
IRRADIANCE; SPECTRAL IRRADIANCE; RADIATIVE OUTPUT; MONITOR TIM;
VARIABILITY; CLIMATE; RECORD
AB During the last decade, observations from SORCE (Solar Radiation and Climate Experiment)/TIM (Total Irradiance Monitor), ACRIMSAT (Active Cavity Radiometer Irradiance Monitor Satellite)/ACRIM III, and SOHO (Solar and Heliospheric Observatory)/VIRGO (Variability of IRradiance and Gravity Oscillations Sun PhotoMeter) provided Total Solar Irradiance (TSI) measurements with unprecedented accuracy and stability to determine the amount of solar irradiance reaching the top of the atmosphere and how solar irradiance varies on different time scales. These three independent measurements are analyzed using the EEMD (Ensemble Empirical Mode Decomposition) method to characterize the phase and amplitude of the 27-day solar rotational variation in TSI. The mode decomposition clearly identifies a 27-day solar rotational signature on TSI measurements. The rotational variations of TSI from the three independent observations are generally consistent with each other, despite different mean TSI values. During the declining phase of solar cycle 23, the amplitude of TSI 27-day variations is as high as 0.8 W/m(2) (similar to 0.05%), while during the rising phase of solar cycle 24, the amplitude is up to 0.4 W/m(2) (similar to 0.04%). During the minimum phase (2008-2009), the amplitude of the rotational mode is only similar to 0.1 W/m(2). The correlation of this rotational mode between TIM and ACRIM III is similar to 0.92 and the slope of the local peak values is similar to 0.98. The correlation between TIM and VIRGO is similar to 0.96 and the slope of the local peak values is similar to 0.98, very similar to the slope with ACRIM III. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Lee, Jae N.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Lee, Jae N.; Cahalan, Robert F.; Wu, Dong L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lee, JN (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
EM jae.n.lee@nasa.gov
RI Wu, Dong/D-5375-2012
FU NASA Living With a Star Targeted Research and Technology Program
[NNH1OZDA001]
FX We thank two anonymous reviewers whose detailed and specific comments
contributed significantly to improving the paper. This work is supported
by the NASA Living With a Star Targeted Research and Technology Program
(NNH1OZDA001). We also thank the SORCE, ACRIM III, VIRGO teams for
providing their data and analysis support.
NR 40
TC 4
Z9 4
U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
EI 1879-1824
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD SEP
PY 2015
VL 132
BP 64
EP 73
DI 10.1016/j.jastp.2015.07.001
PG 10
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA CO4YT
UT WOS:000359167500007
ER
PT J
AU Chen, Y
Yuan, WP
Xia, JZ
Fisher, JB
Dong, WJ
Zhang, XT
Liang, SL
Ye, AZ
Cai, WW
Feng, JM
AF Chen, Yang
Yuan, Wenping
Xia, Jiangzhou
Fisher, Joshua B.
Dong, Wenjie
Zhang, Xiaotong
Liang, Shunlin
Ye, Aizhong
Cai, Wenwen
Feng, Jinming
TI Using Bayesian model averaging to estimate terrestrial
evapotranspiration in China
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Evapotranspiration; Bayesian model averaging; Water balance; Remote
sensing; China
ID ARTIFICIAL NEURAL-NETWORK; NET PRIMARY PRODUCTIVITY; SATELLITE DATA;
MONTHLY INFLOW; WATER-BALANCE; ABSORBED PAR; NORTH CHINA; WIND-SPEED;
FLUX TOWER; MODIS DATA
AB Evapotranspiration (ET) is critical to terrestrial ecosystems as it links the water, carbon, and surface energy exchanges. Numerous ET models were developed for the ET estimations, but there are large model uncertainties. In this study, a Bayesian Model Averaging (BMA) method was used to merge eight satellite-based models, including five empirical and three process-based models, for improving the accuracy of ET estimates. At twenty-three eddy covariance flux towers, we examined the model performance on all possible combinations of eight models and found that an ensemble with four models (BMA_Best) showed the best model performance. The BMA_Best method can outperform the best of eight models, and the Kling-Gupta efficiency (KGE) value increased by 4% compared with the model with the highest KGE, and decreased RMSE by 4%. Although the correlation coefficient of BMA_Best is less than the best single model, the bias of BMA_Best is the smallest compared with the eight models. Moreover, based on the water balance principle over the river basin scale, the validation indicated the BMA_Best estimates can explain 86% variations. In general, the results showed BMA estimates will be very useful for future studies to characterize the regional water availability over long-time series. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Chen, Yang; Yuan, Wenping; Xia, Jiangzhou; Dong, Wenjie; Cai, Wenwen] Beijing Normal Univ, Future Earth Res Inst, State Key Lab Earth Surface Processes & Resource, Beijing 100875, Peoples R China.
[Chen, Yang; Yuan, Wenping; Xia, Jiangzhou; Dong, Wenjie; Cai, Wenwen] Beijing Normal Univ, Future Earth Res Inst, State Key Lab Earth Surface Processes & Resource, Zhuhai 519087, Peoples R China.
[Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, Xiaotong; Liang, Shunlin] Beijing Normal Univ, Sch Geog, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China.
[Liang, Shunlin] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Ye, Aizhong] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China.
[Feng, Jinming] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Reg Climate Environm Res Temperate East A, Beijing 100029, Peoples R China.
RP Yuan, WP (reprint author), Beijing Normal Univ, Future Earth Res Inst, State Key Lab Earth Surface Processes & Resource, Beijing 100875, Peoples R China.
EM yuanwpcn@l26.com
RI liang, shunlin/C-2809-2015;
OI ye, aizhong/0000-0002-5272-134X; Fisher, Joshua/0000-0003-4734-9085
FU National Science Foundation for Excellent Young Scholars of China
[41322005]; National High Technology Research and Development Program of
China (863 Program) [2013AA122003]; State Key Laboratory of
Environmental Change and Natural Disaster [2015jzhz03]; Program for New
Century Excellent Talents in University [NCET-12-0060]
FX This study was supported by the National Science Foundation for
Excellent Young Scholars of China (41322005), the National High
Technology Research and Development Program of China (863 Program)
(2013AA122003), State Key Laboratory of Environmental Change and Natural
Disaster (2015jzhz03) and Program for New Century Excellent Talents in
University (NCET-12-0060). We thank the Coordinated Observations and
Integrated Research over Arid and Semi-arid China (COIRAS) for providing
the eddy covariance flux data. We also acknowledge all the principal
investigators, AsiaFlux and ChinaFlux for their volunteer contribution
for data distribution. We thank Takahisa Maeda and Samreong Panuthai for
providing the data of ID-Bks and TL-Skr in AsiaFlux. This study uses the
LandFlux-EVAL merged benchmark synthesis products of ETH Zurich produced
under the aegis of the GEWEX and ILEAPS projects
(http://www.iac.ethz.ch/url/research/LandFlux-EVAL/). We thank Jun
Asanuma, Shiping Chen, Shijie Han, Huizhi Liu, Shihua Lu, Akira Miyata,
Zhuguo Ma, Takeshi Ohta, Jianwei Tang, Runyuan Wang, Shaoqiang Wang,
Tianbao Zhao and Tonggang Zha for using their monitoring data.
NR 98
TC 1
Z9 2
U1 6
U2 44
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 SEP
PY 2015
VL 528
BP 537
EP 549
DI 10.1016/j.jhydrol.2015.06.059
PG 13
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA CO2EG
UT WOS:000358968200044
ER
PT J
AU Zubieta, R
Getirana, A
Espinoza, JC
Lavado, W
AF Zubieta, Ricardo
Getirana, Augusto
Espinoza, Jhan Carlo
Lavado, Waldo
TI Impacts of satellite-based precipitation datasets on rainfall-runoff
modeling of the Western Amazon basin of Peru and Ecuador
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Hydrological modeling; Precipitation dataset; Satellite; Western Amazon
basin; Andean-Amazon regions
ID MEASURING MISSION TRMM; TROPICAL RAINFALL; INTERANNUAL VARIABILITY;
AUTOMATIC CALIBRATION; TEMPORAL RESOLUTION; GLOBAL OPTIMIZATION;
WATER-BALANCE; ANALYSIS TMPA; RIVER-BASIN; ALGORITHM
AB Satellites are an alternative source of rainfall data used as input to hydrological models in poorly gauged or ungauged regions. They are also useful in regions with highly heterogeneous precipitation, such as the tropical Andes. This paper evaluates three satellite precipitation datasets (TMPA, CMORPH, PERSIANN), as well as a dataset based only on rain gauge data (HYBAM), and their impacts on the water balance of the Western Amazon basin, a region where hydrological modeling and hydrological forecasting are poorly developed. These datasets were used as inputs in the MGB-IPH hydrological model to simulate streamflows for the 2003-2009 period. The impacts of precipitation on model parameterization and outputs were evaluated in two calibration experiments. In Experiment 1, parameter sets were separately defined for each catchment; in Experiment 2, a single parameter set was defined for the entire basin. TMPA shows overestimated precipitation over the northern region, while CMORPH and PERSIANN significantly underestimate rainfall in the same that region and along the Andes. TMPA and CMORPH lead to similar estimates of mean evapotranspiration (similar to 2 mm/day) for different regions along the entire basin, while PERSIANN is the least accurate (similar to 0.5 mm/day). Overall, better scores for streamflow simulations are obtained with Experiment 1 forced by HYBAM and TMPA. Nevertheless, results using the three satellite datasets indicate inter-basin differences, low performance in the northern and high in the southern regions. Low model performances are mainly related to scale issues and forcing errors in small basins over regions that present very low rainfall seasonality. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Zubieta, Ricardo; Espinoza, Jhan Carlo] IGP, Lima, Peru.
[Getirana, Augusto] NASA, Goddard Hydrol Sci Lab, Greenbelt, MD USA.
[Getirana, Augusto] Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA.
[Zubieta, Ricardo; Espinoza, Jhan Carlo; Lavado, Waldo] Univ Nacl Agraria Molina, Lima, Peru.
[Lavado, Waldo] SENAMHI, Lima, Peru.
RP Zubieta, R (reprint author), IGP, Lima, Peru.
EM ricardo.zubieta@igp.gob.pe
RI Espinoza, Jhan Carlo/A-9396-2011; Zubieta, Ricardo/E-9880-2016
OI Espinoza, Jhan Carlo/0000-0001-7732-8504; Zubieta,
Ricardo/0000-0002-4315-7695
FU PNICP-Peru [397-PNICP-PIAP-2014]
FX The authors would like to thank SO-HYBAM for providing the precipitation
dataset, and M. Saavedra, J. Quijano and S. Chavez (IGP) for their
support in data preprocessing. The study benefitted from maps made
available by the Ministerio de Medio Ambiente (Ecuador), Sociedad
Ecuatoriana de la Ciencia del Suelo (SECS-Ecuador), Instituto Geografico
Agustin Codazzi (IGAC-Colombia) and the former Instituto Nacional de
Recursos Naturales (INRENA-Peru). The authors also would like to
acknowledge GSFC/DAAC, NASA for providing TMPA data
(http://disc.sci.gsfc.nasa.gov/ /data/TRMM/Gridded/), the NOAA Climate
Prediction Center for providing CMORPH data
(ftp://ftp.cpc.ncep.noaa.gov/precip/global_CMORPH) and the Center for
Hydrometeorolgy & Remote Sensing and the University of California for
providing PERSIANN data
(ftp://persiann.eng.uci.edu/pub/PERSIANN/tar_6hr/). Suggestions from K.
Takahashi, B. Fraser, P. Lagos and H. Segura were greatly appreciated.
We also thank the PNICP-Peru for providing funds through the 'contrato
No397-PNICP-PIAP-2014' contract.
NR 79
TC 3
Z9 4
U1 0
U2 12
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 SEP
PY 2015
VL 528
BP 599
EP 612
DI 10.1016/j.jhydrol.2015.06.064
PG 14
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA CO2EG
UT WOS:000358968200049
ER
PT J
AU Manns, HR
Berg, AA
Colliander, A
AF Manns, Hida R.
Berg, Aaron A.
Colliander, Andreas
TI Soil organic carbon as a factor in passive microwave retrievals of soil
water content over agricultural croplands
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Passive microwave remote sensing; Brightness temperature; Soil organic
carbon; Soil water content; SMAP satellite; Soil dielectric constant
ID EXPERIMENT 2012 SMAPVEX12; ACTIVE L-BAND; DIELECTRIC-CONSTANT; SIZE
DISTRIBUTION; MOIST SOILS; MATTER; MODEL; VALIDATION; SENSOR;
POLARIZATION
AB Remote sensing has the potential to deliver global soil water content (SWC) on vast scales with frequent revisit times for progress in the fields of climate, weather forecasting, agriculture and hydrology. Although surface roughness, vegetation and soil texture have been established as sources of variability in passive microwave interpretation, soil organic carbon (SOC) has not typically been considered as a factor that affects SWC estimation during field sampling campaigns. SOC was observed along with soil texture and bulk density during the Soil Moisture Active Passive Validation Experiment in 2012 (SMAPVEX12), the Soil Moisture Active Passive (SMAP) satellite algorithm development field sampling campaign held June 6 to July 19 in Southern Manitoba, Canada. Aerial measurements from the PALS (Passive Active L-band System) instrument were recorded over agricultural fields and forest areas from aircraft while SWC was measured simultaneously on the ground with resistance probes on 17 sampling dates. Additionally, fields were sampled for surface roughness, vegetation growth and water content, soil and vegetation temperature and soil physical characteristics. A soil core was collected on each field each sampling time to assess bulk density, soil particle size and SOC. SOC accounted for more variability in the anomalies between PALS and ground sampled SWC than sand, clay or bulk density, although all soil variables explained significant variability. With analysis by partial least squares multiple regression over 11 sampling dates and 39 fields where both ground and PALS data were well represented, only SOC contributed significantly to the regression of SWC beyond the variance all soil variables had in common. The significance of SOC in the relative SWC anomalies was highest in very wet and very dry conditions and in loam soil over all sampling dates, while bulk density was more significant in sand soils. This analysis suggests SOC is a simple variable that incorporates multiple aspects of soil hydrology and may improve the algorithms for remotely sensing estimation of SWC in various landscapes. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Manns, Hida R.; Berg, Aaron A.] Univ Guelph, Dept Geog, Guelph, ON NOG 2W1, Canada.
[Colliander, Andreas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Berg, AA (reprint author), Univ Guelph, Dept Geog, Guelph, ON NOG 2W1, Canada.
EM aberg@uoguelph.ca
FU Natural Science and Engineering Research Council of Canada; Canadian
Space Agency
FX Thanks to the entire SMAPVEX12 team for the success of this extensive
research. In particular, our sincere appreciation is extended to Rebecca
Warren for processing the soil carbon samples, and Professor Paul
Bullock and students and Tracy Rowlandson for the soil and SWC data
preparation. We also thank Adam Bonnycastle for GIS expertise and Marie
Puddister for mapping assistance in the department of Geography,
University of Guelph. We also wish to thank the anonymous reviewers for
their constructive feedback used to improve this manuscript. Funding
from the Natural Science and Engineering Research Council of Canada and
Canadian Space Agency is gratefully acknowledged. Part of this work was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology under contract with the National Aeronautics and Space
Administration.
NR 52
TC 3
Z9 3
U1 12
U2 45
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 SEP
PY 2015
VL 528
BP 643
EP 651
DI 10.1016/j.jhydrol.2015.06.058
PG 9
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA CO2EG
UT WOS:000358968200053
ER
PT J
AU Sabra, MS
AF Sabra, Mohammad S.
TI Geant4 validation of neutron production on thick targets bombarded with
120 GeV protons
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article
DE Geant4; Proton reaction; Thick target; Neutron production
ID MULTIPLICITY DISTRIBUTIONS; SPALLATION REACTIONS; ENERGY
AB Neutron energy spectra and angular distributions are calculated for 120 GeV protons on thick graphite, aluminum, copper, and tungsten targets using relevant physics models within the Monte-Carlo simulation package Geant4. The calculations are compared to data from recent experiment. Discrepancies are observed between experimental data and Geant4 models, and suggest that improvements of the intra-(INC) and inter-nuclear cascade processes employed by the models are required. (C) 2015 Elsevier B.V. All rights reserved.
C1 George C Marshall Space Flight Ctr, NASA Postdoctoral Program, Huntsville, AL 35805 USA.
RP Sabra, MS (reprint author), George C Marshall Space Flight Ctr, NASA Postdoctoral Program, Huntsville, AL 35805 USA.
EM mohammad.s.sabra@nasa.gov
FU appointment to the NASA Postdoctoral Program at Marshall Space Flight
Center; NASA
FX The author would like to thank Dr.Kajimoto for providing us with the
experimental data in numerical form. This work was supported by an
appointment to the NASA Postdoctoral Program at Marshall Space Flight
Center, administered by Oak Ridge Associated Universities through a
contract with NASA.
NR 11
TC 1
Z9 2
U1 0
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
EI 1872-9584
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD SEP 1
PY 2015
VL 358
BP 245
EP 250
DI 10.1016/j.nimb.2015.06.016
PG 6
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA CO5AA
UT WOS:000359170800038
ER
PT J
AU Devaraju, N
Bala, G
Nemani, R
AF Devaraju, N.
Bala, G.
Nemani, R.
TI Modelling the influence of land-use changes on biophysical and
biochemical interactions at regional and global scales
SO PLANT CELL AND ENVIRONMENT
LA English
DT Review
DE atmospheric circulation; biochemical and biophysical processes; climate
change
ID CARBON-ISOTOPE DISCRIMINATION; GENERAL-CIRCULATION MODEL; TROPICAL
DEFORESTATION; COVER CHANGE; CLIMATE-CHANGE; ATMOSPHERIC CIRCULATION;
AMAZONIAN DEFORESTATION; TERRESTRIAL CARBON; MISSISSIPPI RIVER; SURFACE
ALBEDO
AB Land-use changes since the start of the industrial era account for nearly one-third of the cumulative anthropogenic CO2 emissions. In addition to the greenhouse effect of CO2 emissions, changes in land use also affect climate via changes in surface physical properties such as albedo, evapotranspiration and roughness length. Recent modelling studies suggest that these biophysical components may be comparable with biochemical effects. In regard to climate change, the effects of these two distinct processes may counterbalance one another both regionally and, possibly, globally. In this article, through hypothetical large-scale deforestation simulations using a global climate model, we contrast the implications of afforestation on ameliorating or enhancing anthropogenic contributions from previously converted (agricultural) land surfaces. Based on our review of past studies on this subject, we conclude that the sum of both biophysical and biochemical effects should be assessed when large-scale afforestation is used for countering global warming, and the net effect on global mean temperature change depends on the location of deforestation/afforestation. Further, although biochemical effects trigger global climate change, biophysical effects often cause strong local and regional climate change. The implication of the biophysical effects for adaptation and mitigation of climate change in agriculture and agroforestry sectors is discussed.
center dot Land-use changes affect global and regional climates through both biochemical and biophysical process. center dot Climate effect from biophysical process depends on the location of land-use change. center dot Climate mitigation strategies such as afforestation/reforestation should consider the net effect of biochemical and biophysical processes for effective mitigation. center dot Climate-smart agriculture could use bio-geoengineering techniques that consider plant biophysical characteristics such as reflectivity and water use efficiency.
C1 [Devaraju, N.; Bala, G.] Indian Inst Sci, Divecha Ctr Climate Change, Bangalore 560012, Karnataka, India.
[Devaraju, N.; Bala, G.] Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
[Nemani, R.] NASA, Ames Res Ctr, Ecol Forecasting Lab, Moffett Field, CA 94035 USA.
RP Devaraju, N (reprint author), Indian Inst Sci, Divecha Ctr Climate Change, Bangalore 560012, Karnataka, India.
EM dev@caos.iisc.ernet.in
OI Devaraju, Narayanappa/0000-0001-8471-3961
FU Department of Science and Technology [DST0948]; Divecha Center for
Climate Change; FIST; Department of Science and Technology
FX We thank the funding from Department of Science and Technology under the
grant DST0948. Dr Devaraju is supported by the Divecha Center for
Climate Change. Computations were carried out at CAOS HPC facility
funded by FIST, Department of Science and Technology and Divecha Center
for Climate Change. We also thank the anonymous reviewers and the
associate editor Dr Danielle Way for their comments and suggestions that
helped us to improve the original manuscript.
NR 112
TC 12
Z9 12
U1 8
U2 53
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0140-7791
EI 1365-3040
J9 PLANT CELL ENVIRON
JI Plant Cell Environ.
PD SEP
PY 2015
VL 38
IS 9
SI SI
BP 1931
EP 1946
DI 10.1111/pce.12488
PG 16
WC Plant Sciences
SC Plant Sciences
GA CO7VT
UT WOS:000359371800019
PM 25410808
ER
PT J
AU Yoshida, Y
Joiner, J
Tucker, C
Berry, J
Lee, JE
Walker, G
Reichle, R
Koster, R
Lyapustin, A
Wang, Y
AF Yoshida, Y.
Joiner, J.
Tucker, C.
Berry, J.
Lee, J. -E.
Walker, G.
Reichle, R.
Koster, R.
Lyapustin, A.
Wang, Y.
TI The 2010 Russian drought impact on satellite measurements of
solar-induced chlorophyll fluorescence: Insights from modeling and
comparisons with parameters derived from satellite reflectances
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Vegetation; Drought; Chlorophyll; Vegetation index; NDVI; MODIS;
Fluorescence; GOME-2; APAR; FPAR; Gross primary productivity
ID SUN-INDUCED FLUORESCENCE; VEGETATION PHENOLOGY; SEASONAL CYCLE; ABSORBED
PAR; LEAF-AREA; SPACE; RETRIEVAL; MODIS; GOSAT; PHOTOSYNTHESIS
AB We examine satellite-based measurements of solar-induced chlorophyll fluorescence (SIF) over the region impacted by the Russian drought and heat wave of 2010. Like the popular Normalized Difference Vegetation Index (NDVI) that has been used for decades to measure photosynthetic capacity, SIF measurements are sensitive to the fraction of absorbed photosynthetically-active radiation (fPAR). However, in addition, SIF is sensitive to PAR as well as the fluorescence yield that is related to the photosynthetic yield. Both SIF and NDVI from satellite data show drought-related declines early in the growing season in 2010 as compared to other years between 2007 and 2013 for areas dominated by crops and grasslands. This suggests an early manifestation of the dry conditions on fPAR. Using MODIS fPAR retrievals, we computed SIF/APAR which is related to light use efficiencies (LUEs) for fluorescence and photosynthesis. We found drought-related losses in fluorescence efficiency for all areas including those dominated by mixed forests. Unlike croplands and grasslands, areas of mixed forest did not show significant drought-related declines in fPAR. We also simulated SIF and Gross Primary Productivity (GPP) using a global land surface model driven by observation-based meteorological fields. The model provides a reasonable simulation of the drought and heat impacts on SIF in terms of the spatial extents of anomalies, but some differences were found in timing of the peak drought response between modeled and observed SIP. Model data also suggested that drought-related declines in LUE for fluorescence and photosynthesis in areas of mixed forest produce losses in SIF and GPP. SIF and GPP losses due to drought in croplands and grasslands result from both LUE and fPAR reductions. The combination of SIF and NDVI or fPAR data is shown to be an important source of information for evaluating model performance. (C) 2015 Elsevier Inc All rights reserved.
C1 [Yoshida, Y.; Joiner, J.; Tucker, C.; Reichle, R.; Koster, R.; Lyapustin, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yoshida, Y.; Walker, G.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Berry, J.] Carnegie Inst Sci, Stanford, CA USA.
[Lee, J. -E.] Brown Univ, Providence, RI 02912 USA.
[Wang, Y.] Univ Maryland, Joint Ctr Environm Technol, Baltimore, MD USA.
RP Yoshida, Y (reprint author), NASA, Goddard Space Flight Ctr, Code 614, Greenbelt, MD 20771 USA.
EM yasuko.yoshida-1@nasa.gov
RI Koster, Randal/F-5881-2012; Reichle, Rolf/E-1419-2012
OI Koster, Randal/0000-0001-6418-6383;
NR 62
TC 10
Z9 10
U1 13
U2 64
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 1
PY 2015
VL 166
BP 163
EP 177
DI 10.1016/j.rse.2015.06.008
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CN7RU
UT WOS:000358632500014
ER
PT J
AU Hilker, T
Lyapustin, AI
Hall, FG
Myneni, R
Knyazikhin, Y
Wang, YJ
Tucker, CJ
Sellers, PJ
AF Hilker, Thomas
Lyapustin, Alexei I.
Hall, Forrest G.
Myneni, Ranga
Knyazikhin, Yuri
Wang, Yujie
Tucker, Compton J.
Sellers, Piers J.
TI On the measurability of change in Amazon vegetation from MODIS
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE MODIS; Amazon; MAIAC; Sensitivity analysis; Vegetation change; MOD09
ID FORESTS GREEN-UP; ATMOSPHERIC CORRECTION; DRY SEASON; REFLECTANCE
PRODUCTS; TROPICAL FOREST; CLIMATE-CHANGE; RAIN-FORESTS; CLOUD COVER;
DEFORESTATION; DROUGHT
AB The Amazon rainforest is a critical hotspot for bio-diversity, and plays an essential role in global carbon, water and energy fluxes and the earth's climate. Our ability to project the role of vegetation carbon feedbacks on future climate critically depends upon our understanding of this tropical ecosystem, its tolerance to climate extremes and tipping points of ecosystem collapse. Satellite remote sensing is the only practical approach to obtain observational evidence of trends and changes across large regions of the Amazon forest; however, inferring these trends in the presence of high cloud cover fraction and aerosol concentrations has led to widely varying conclusions. Our study provides a simple and direct statistical analysis of a measurable change in daily and composite surface reflectance obtained from the Moderate Resolution Imaging Spectroradiometer (MODIS) based on the noise level of data and the number of available observations. Depending on time frame and data product chosen for analysis, changes in leaf area need to exceed up to 2 units leaf area per unit ground area (expressed as m(2) m(-2)) across much of the basin before these changes can be detected at a 95% confidence level with conventional approaches, roughly corresponding to a change in NDVI and EVI of about 25%. A potential way forward may be provided by advanced multi-angular techniques, such as the Multi-Angle Implementation of Atmospheric Correction Algorithm (MAIAC), which allowed detection of changes of about 0.6-0.8 units in leaf area (2-6% change in NDVI) at the same confidence level. In our analysis, the use of the Enhanced Vegetation Index (EVI) did not improve accuracy of detectable change in leaf area but added a complicating sensitivity to the bidirectional reflectance, or view geometry effects. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Hilker, Thomas] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA.
[Lyapustin, Alexei I.; Hall, Forrest G.; Wang, Yujie; Tucker, Compton J.; Sellers, Piers J.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hall, Forrest G.; Wang, Yujie] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Myneni, Ranga; Knyazikhin, Yuri] Boston Univ Earth & Environm, Boston, MA 02215 USA.
RP Hilker, T (reprint author), Oregon State Univ, Coll Forestry, 231 Peavy Hall, Corvallis, OR 97331 USA.
EM thomas.hilker@oregonstate.edu
RI Myneni, Ranga/F-5129-2012
FU NASA Science of Terra and Aqua program
FX We are grateful to the NASA Center for Climate Simulation (NCCS) for
computational support and access to their high performance cluster.
MAIAC data for the amazon basin are available at
ftp://maiac@dataportal.nccs.nasa.gov/DataRelease/SouthAmerica. Support
for Drs. Lyapustin and Wang was provided by the NASA Science of Terra
and Aqua program.
NR 48
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U2 67
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD SEP 1
PY 2015
VL 166
BP 233
EP 242
DI 10.1016/j.rse.2015.05.020
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CN7RU
UT WOS:000358632500019
ER
PT J
AU Juarez, PD
Leckey, CAC
AF Juarez, Peter D.
Leckey, Cara A. C.
TI Multi-frequency local wavenumber analysis and ply correlation of
delamination damage
SO ULTRASONICS
LA English
DT Article; Proceedings Paper
CT 2015 International Congress on Ultrasonics (ICU)
CY MAY 11-14, 2015
CL Metz, FRANCE
DE Guided waves; Wavenumber; Composite; De lamination; Laser vibrometer
ID COMPOSITE PLATES; IMPACT DAMAGE; GUIDED-WAVES
AB Wavenumber domain analysis through use of scanning laser Doppler vibrometry has been shown to be effective for non-contact inspection of damage in composites. Qualitative and semi-quantitative local wavenumber analysis of realistic delamination damage and quantitative analysis of idealized damage scenarios (Teflon inserts) have been performed previously in the literature. This paper presents a new methodology based on multi-frequency local wavenumber analysis for quantitative assessment of multi-ply delamination damage in carbon fiber reinforced polymer (CFRP) composite specimens. The methodology is presented and applied to a real world damage scenario (impact damage in an aerospace CFRP composite). The methodology yields delamination size and also correlates local wavenumber results from multiple excitation frequencies to theoretical dispersion curves in order to robustly determine the delamination ply depth. Results from the wavenumber based technique are validated against a traditional nondestructive evaluation method. Published by Elsevier B.V.
C1 [Juarez, Peter D.; Leckey, Cara A. C.] NASA, Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23681 USA.
RP Leckey, CAC (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM cara.ac.leckey@nasa.gov
NR 29
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U1 0
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0041-624X
EI 1874-9968
J9 ULTRASONICS
JI Ultrasonics
PD SEP
PY 2015
VL 62
BP 56
EP 65
DI 10.1016/j.ultras.2015.05.001
PG 10
WC Acoustics; Radiology, Nuclear Medicine & Medical Imaging
SC Acoustics; Radiology, Nuclear Medicine & Medical Imaging
GA CO2EO
UT WOS:000358969100008
PM 25980617
ER
PT J
AU Yu, LY
Tian, ZH
Leckey, CAC
AF Yu, Lingyu
Tian, Zhenhua
Leckey, Cara A. C.
TI Crack imaging and quantification in aluminum plates with guided wave
wavenumber analysis methods
SO ULTRASONICS
LA English
DT Article; Proceedings Paper
CT 2015 International Congress on Ultrasonics (ICU)
CY MAY 11-14, 2015
CL Metz, FRANCE
DE Guided waves; Wavenumber analysis; Guided wave imaging; Crack detection;
Aluminum plate
ID FINITE INTEGRATION TECHNIQUE; LAMB WAVES; METALLIC STRUCTURES; DAMAGE
DETECTION; DEFECT DETECTION; SENSOR NETWORK; MODE; ARRAY; DECOMPOSITION;
PROPAGATION
AB Guided wavefield analysis methods for detection and quantification of crack damage in an aluminum plate are presented in this paper. New wavenumber components created by abrupt wave changes at the structural discontinuity are identified in the frequency-wavenumber spectra. It is shown that the new wavenumbers can be used to detect and characterize the crack dimensions. Two imaging based approaches, filter reconstructed imaging and spatial wavenumber imaging, are used to demonstrate how the cracks can be evaluated with wavenumber analysis. The filter reconstructed imaging is shown to be a rapid method to map the plate and any existing damage, but with less precision in estimating crack dimensions; while the spatial wavenumber imaging provides an intensity image of spatial wavenumber values with enhanced resolution of crack dimensions. These techniques are applied to simulated wavefield data, and the simulation based studies show that spatial wavenumber imaging method is able to distinguish cracks of different seventies. Laboratory experimental validation is performed for a single crack case to confirm the methods' capabilities for imaging cracks in plates. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Yu, Lingyu; Tian, Zhenhua] Univ S Carolina, Dept Mech Engn, Columbia, SC 29208 USA.
[Leckey, Cara A. C.] NASA, Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23665 USA.
RP Tian, ZH (reprint author), Univ S Carolina, Dept Mech Engn, Columbia, SC 29208 USA.
EM tianz@email.sc.edu
RI Tian, Zhenhua/I-6687-2015
OI Tian, Zhenhua/0000-0002-1903-5604
FU SC NASA EPSCoR Research and Education Awards Program (REAP)
[21-NE-USC_Yu-RGP]
FX The authors would like to acknowledge and thank (1) the
non-reimbursement Space Act Umbrella Agreement SAA1-1181 between South
Carolina Research Foundation (SCRF) and the National Aeronautics and
Space Administration (NASA) Langley Research Center, (2) University of
South Carolina SPARC graduate fellowship, and (3) SC NASA EPSCoR
Research and Education Awards Program (REAP) 21-NE-USC_Yu-RGP.
NR 66
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U1 1
U2 16
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0041-624X
EI 1874-9968
J9 ULTRASONICS
JI Ultrasonics
PD SEP
PY 2015
VL 62
BP 203
EP 212
DI 10.1016/j.ultras.2015.05.019
PG 10
WC Acoustics; Radiology, Nuclear Medicine & Medical Imaging
SC Acoustics; Radiology, Nuclear Medicine & Medical Imaging
GA CO2EO
UT WOS:000358969100025
PM 26049731
ER
PT J
AU de Foy, B
Lu, ZF
Streets, DG
Lamsal, LN
Duncan, BN
AF de Foy, Benjamin
Lu, Zifeng
Streets, David G.
Lamsal, Lok N.
Duncan, Bryan N.
TI Estimates of power plant NOx emissions and lifetimes from OMI NO2
satellite retrievals
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Emission inventory; Satellite retrieval; OMI; CEMS; Power plant NOx;
Chemical lifetime
ID OZONE MONITORING INSTRUMENT; TROPOSPHERIC NO2; UNITED-STATES;
NITROGEN-OXIDES; AIR-QUALITY; ATMOSPHERIC COMPOSITION; IN-SITU; SPACE;
POLLUTION; SO2
AB Isolated power plants with well characterized emissions serve as an ideal test case of methods to estimate emissions using satellite data. In this study we evaluate the Exponentially-Modified Gaussian (EMG) method and the box model method based on mass balance for estimating known NOx emissions from satellite retrievals made by the Ozone Monitoring Instrument (OMI). We consider 29 power plants in the USA which have large NOx plumes that do not overlap with other sources and which have emissions data from the Continuous Emission Monitoring System (CEMS). This enables us to identify constraints required by the methods, such as which wind data to use and how to calculate background values. We found that the lifetimes estimated by the methods are too short to be representative of the chemical lifetime. Instead, we introduce a separate lifetime parameter to account for the discrepancy between estimates using real data and those that theory would predict. In terms of emissions, the EMG method required averages from multiple years to give accurate results, whereas the box model method gave accurate results for individual ozone seasons. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [de Foy, Benjamin] St Louis Univ, Dept Earth & Atmospher Sci, St Louis, MO 63103 USA.
[Lu, Zifeng; Streets, David G.] Argonne Natl Lab, Div Energy Syst, Argonne, IL 60439 USA.
[Lamsal, Lok N.; Duncan, Bryan N.] NASA Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA.
RP de Foy, B (reprint author), St Louis Univ, Dept Earth & Atmospher Sci, St Louis, MO 63103 USA.
EM bdefoy@slu.edu
RI de Foy, Benjamin/A-9902-2010; Duncan, Bryan/A-5962-2011
OI de Foy, Benjamin/0000-0003-4150-9922;
FU NASA Air Quality Applied Sciences Team (AQAST) program, NASA
[NNX11AJ63G]
FX This research was funded by the NASA Air Quality Applied Sciences Team
(AQAST) program, NASA grant #NNX11AJ63G, including funding for the AQAST
Tiger Team "Relationships and trends among satellite NO2
columns, NO emissions, and air quality in North America." We are
grateful for valuable comments and discussion from the team members and
the team leader and assistant leader, Daniel J. Jacob and Tracey
Holloway. We thank the anonymous reviewers for their comments which have
helped improve the paper.
NR 43
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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 SEP
PY 2015
VL 116
BP 1
EP 11
DI 10.1016/j.atmosenv.2015.05.056
PG 11
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA CN5KX
UT WOS:000358469300001
ER
PT J
AU Prouve, T
Duband, L
Hodis, J
Bock, JJ
Bradford, CM
Holmes, W
AF Prouve, T.
Duband, L.
Hodis, J.
Bock, J. J.
Bradford, C. Matt
Holmes, W.
TI SPICA/BLISS cryo-chain demonstrator
SO CRYOGENICS
LA English
DT Article
DE Astrophysics; Sub-Kelvin; Space; SPICA; Sorption-cooler; ADR
ID SPICA; SPECTROMETER; DESIGN; COOLER
AB The Background Limited Infrared Submillimeter Spectrometer (BLISS) is an instrument proposed for SPICA, the Japanese-European space-borne telescope mission under study for a possible launch in the next decade. The BLISS concept is a suite of aluminum spectrometer modules totaling similar to 10 kg cooled to 50 mK. Cooling this ambitious instrument with high-duty cycle within the stringent heat-rejection allocations envisioned for SPICA is a challenge. We have developed a solution consisting of two stages: (1) a continuous 300 mK intercept stage provided by two 3He sorption coolers operated sequentially, and (2) a 50 mK adiabatic demagnetization refrigerator (ADR) operated in single-shot mode. We have built a prototype cooler and demonstrated it in a dedicated SPICA-like thermal testbed with regulated stages enabling measurement of rejected heat at 1.7 K and 4.5 K. The approach offers lower mass than a dual-stage ADR, and lower rejected power to 1.7 K and 4.5 K than a comparable single-shot 300 mK system, while insuring a high duty cycle. As a demonstration of feasibility for SPICA and future cryogenic missions, we show long-term cooling with flight-like parasitics at 50 mK and 300 mK requiring only 3 mW and 8 mW rejected at 1.7 K and 4.5 K, respectively. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Prouve, T.; Bock, J. J.; Bradford, C. Matt] CALTECH, Dept Phys & Astron, Pasadena, CA 91106 USA.
[Hodis, J.; Bock, J. J.; Bradford, C. Matt; Holmes, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Prouve, T.; Duband, L.] Univ Grenoble Alpes, CEA INAC SBT, F-38000 Grenoble, France.
RP Prouve, T (reprint author), Univ Grenoble Alpes, CEA INAC SBT, F-38000 Grenoble, France.
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. We acknowledge Adrian Lee for
lending the ADR magnet and salt pill used for this test.
NR 11
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U1 3
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0011-2275
EI 1879-2235
J9 CRYOGENICS
JI Cryogenics
PD SEP
PY 2015
VL 70
BP 70
EP 75
DI 10.1016/j.cryogenics.2015.06.001
PG 6
WC Thermodynamics; Physics, Applied
SC Thermodynamics; Physics
GA CO0DN
UT WOS:000358820400010
ER
PT J
AU Lagomasino, D
Price, RM
Herrera-Silveira, J
Miralles-Wilhelm, F
Merediz-Alonso, G
Gomez-Hernandez, Y
AF Lagomasino, David
Price, Rene M.
Herrera-Silveira, Jorge
Miralles-Wilhelm, Fernando
Merediz-Alonso, Gonzalo
Gomez-Hernandez, Yadira
TI Connecting Groundwater and Surface Water Sources in Groundwater
Dependent Coastal Wetlands and Estuaries: Sian Ka'an Biosphere Reserve,
Quintana Roo, Mexico
SO ESTUARIES AND COASTS
LA English
DT Article
DE Groundwater discharge; Oligotrophic; Eutrophic; Phosphorus; Mangroves;
Hypersaline
ID MODELING STREAMWATER CHEMISTRY; SOILWATER END-MEMBERS; MANGROVE TIDAL
CREEK; YUCATAN PENINSULA; CHICXULUB IMPACT; MIXING ZONE; NATURAL-WATERS;
PHOSPHORUS; AQUIFER; DISSOLUTION
AB Groundwater and surface water samples were collected in five different regions of the Sian Ka'an Biosphere Reserve (SKBR) along the eastern coast of the Yucatan Peninsula in Quintana Roo, Mexico. Samples were analyzed for major ions, total phosphorus, total nitrogen, delta O-18, and delta H-2. Chemical modeling and a coupled principal component analysis and end-member mixing model were used to identify three groundwater sources that discharge to the coastal wetlands and estuaries of the SKBR. A sulfate-dominated and a calcium-dominated fresh groundwater source were found to contribute significantly to the headwaters of a southern and northern SKBR estuary, respectively. In the northern part of the Reserve, an elevated road disrupts the flow of freshwater through the estuarine zone creating hypersaline conditions and mangrove dead-zones. In a more pristine estuary to the south, coastal groundwater discharge associated with petens (tree islands) accounted for similar to 20 % of the surface water in the mid-estuary. This coastal groundwater discharge from the petens adds a significant amount of phosphorus to the surface water in the estuary relative to the upstream and downstream sources. The lower alkalinity measured in the surface water relative to the high-alkalinity groundwater, despite clear indication of groundwater discharge, suggests that inorganic carbon export through degassing of CO2 could represent important carbon process in mangrove ecosystems. Our results indicate an important groundwater discharge mechanism that may facilitate nutrient delivery to karstic, oligotrophic estuaries when upland and marine nutrient supplies are depleted.
C1 [Lagomasino, David; Price, Rene M.; Miralles-Wilhelm, Fernando] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA.
[Lagomasino, David; Price, Rene M.] Florida Int Univ, Southeast Environm Res Ctr, Miami, FL 33199 USA.
[Herrera-Silveira, Jorge] CINVESTAV IPN, Unidad Merida, Merida 97310, Yucatan, Mexico.
[Merediz-Alonso, Gonzalo] Amigos Sian Kaan, Cancun 77500, Quintana Roo, Mexico.
[Gomez-Hernandez, Yadira] Comis Nacl Areas Nat Protegidas, Cancun 77500, Quintana Roo, Mexico.
RP Lagomasino, D (reprint author), NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA.
EM david.lagomasino@nasa.gov
RI Lagomasino, David/P-8413-2015
OI Lagomasino, David/0000-0003-4008-5363
FU National Science Foundation through the Florida Coastal Everglades
Long-Term Ecological Research program [DBI-0620409]; NASA WaterSCAPES
program [NNX-10AQ13A]; Florida Education Fund McKnight Dissertation Year
Fellowship
FX This research was supported directly by the National Science Foundation
through the Florida Coastal Everglades Long-Term Ecological Research
program under Grant No. DBI-0620409 and the NASA WaterSCAPES program
under Grant No. NNX-10AQ13A. Field and travel support were provided by
the Comision Nacional de Areas Naturales Protegidas (CONANP) and Amigos
de Sian Ka'an in Cancun, Mexico; and the Centro de Investigacion y de
Estudios Avanzados (CINVESTAV) Unidad Merida in Merida, Mexico.
Additional financial support was provided by the Florida Education Fund
McKnight Dissertation Year Fellowship. This is contribution number 690
from the Southeast Environmental Research Center at Florida
International University.
NR 67
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PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1559-2723
EI 1559-2731
J9 ESTUAR COAST
JI Estuaries Coasts
PD SEP
PY 2015
VL 38
IS 5
BP 1744
EP 1763
DI 10.1007/s12237-014-9892-4
PG 20
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA CN7JV
UT WOS:000358611500027
ER
PT J
AU Predoi-Cross, A
Devi, VM
Sung, K
Sinyakova, T
Buldyreva, J
Benner, DC
Smith, MAH
Mantz, AW
AF Predoi-Cross, A.
Devi, V. Malathy
Sung, K.
Sinyakova, T.
Buldyreva, J.
Benner, D. Chris
Smith, M. A. H.
Mantz, A. W.
TI Temperature dependences of N-2-broadening and shift coefficients in the
v(6) perpendicular band of (CH3D)-C-12
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Monodeuterated methane; Infrared spectra; Nitrogen-broadening;
Temperature dependences of widths and shifts; Line mixing; Spectral line
shapes
ID DIODE-LASER MEASUREMENTS; LINE MIXING COEFFICIENTS; 6-10 MU-M;
MULTISPECTRUM ANALYSIS; INFRARED-SPECTRUM; HALF-WIDTHS; NU(3) BAND;
ATMOSPHERIC TEMPERATURES; THEORETICAL CALCULATIONS; FITTING TECHNIQUE
AB The temperature-dependences of line broadening and shift parameters for many (CH3D)-C-12 transitions have been determined using six high-resolution, high signal-to-noise ratio, room-temperature CH3D (98% purity) and CH3D-N-2 spectra recorded with 25 cm path length (at 0.01 cm(-1) unapodized resolution) using the McMath-Pierce FTS located on Kitt Peak, Arizona, and 17 additional high quality, pure CH3D (99% purity) and CH3D-N-2 spectra recorded between 79 and 296 K with the 20.38 cm path coolable cell (at 0.0056 cm(-1) unapodized resolution) with the Bruker 125HR FTS at the Jet Propulsion Laboratory (JPL), Pasadena, California. The spectra have been fitted simultaneously applying a multispectrum nonlinear least-squares technique. In the analysis, the Lorentzian N-2-broadened half-width coefficients and the corresponding pressure-shift coefficients as well as their temperature dependences are extracted for about 400 transitions (0 <= J '' <= 19, K '' <= 16) in the perpendicular (Delta K= +/- 1) v(6) band. At 296 K, the measured N-2-broadened half-width coefficients range from 0.0209 to 0.0782 cm(-1) atm(-1) whereas the majority of the associated N-2-induced shift coefficients are negative, and the values are between -0.016 and 0.005 cm(-1) atm(-1). The temperature dependence exponents for N-2-broadened half-widths range between 0.264 and 0.924, whereas the temperature dependence coefficients for N-2-induced shifts are between 0 and 0.00011 cm(-1) atm(-1) K-1. The N-2-broadened half-width coefficients have been also calculated using a semi-classical approach based on a rigorous treatment of the active molecule as a symmetric top, a model intermolecular potential comprising both short- and long-range interactions, and exact classical trajectories. The role of the various high-order multipoles in the line-broadening at low, middle and high values of the rotational quantum number J '' has been investigated and the main features of the K-dependences analyzed. The calculations performed for 296, 240 and 190 K have allowed to deduce the half-width temperature-dependence exponents, completing the general comparison of our new experimental results with those which are available in the literature. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Predoi-Cross, A.] Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 6R4, Canada.
[Devi, V. Malathy; Benner, D. Chris] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Sung, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sinyakova, T.; Buldyreva, J.] Univ Franche Comte, Inst UTINAM UMR CNRS 6213, F-25030 Besancon, France.
[Smith, M. A. H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
[Mantz, A. W.] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA.
RP Predoi-Cross, A (reprint author), Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 6R4, Canada.
EM adriana.predoicross@uleth.ca
RI Sung, Keeyoon/I-6533-2015
FU National Aeronautics and Space Administration; National Sciences and
Engineering Research Council of Canada; NASA
FX The research described in this article was carried out at the College of
William and Mary, Jet Propulsion Laboratory (JPL), California Institute
of Technology, Connecticut College and NASA Langley Research Center
under contracts with the National Aeronautics and Space Administration.
A. Predoi-Cross acknowledges the support she received from the National
Sciences and Engineering Research Council of Canada and the study leave
program at the University of Lethbridge, AB, Canada for providing the
opportunity to carry out this investigation. The authors thank NASA's
UPPER Atmosphere Research Program for their support of the McMath -
Pierce FTS laboratory.
NR 68
TC 3
Z9 3
U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD SEP
PY 2015
VL 163
BP 120
EP 141
DI 10.1016/j.jqsrt.2015.05.006
PG 22
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA CN7OO
UT WOS:000358624100011
ER
PT J
AU Naughton, F
Keigwin, L
Peteet, D
Costas, S
Desprat, S
Oliveira, D
de Vernal, A
Voelker, A
Abrantes, F
AF Naughton, F.
Keigwin, L.
Peteet, D.
Costas, S.
Desprat, S.
Oliveira, D.
de Vernal, A.
Voelker, A.
Abrantes, F.
TI A 12,000-yr pollen record off Cape Hatteras - Pollen sources and
mechanisms of pollen dispersion
SO MARINE GEOLOGY
LA English
DT Article
DE Eastern North America; Cape Hatteras; Marine pollen signature;
Vegetation changes; Holocene; Land-sea pollen transfer
ID NORTH-ATLANTIC OSCILLATION; WESTERN BOUNDARY CURRENT; SOUTHEASTERN
NEW-YORK; HOLOCENE CLIMATE VARIABILITY; BAY OUTFLOW PLUME; SEA-LEVEL
CHANGES; CHESAPEAKE BAY; COASTAL-PLAIN; UNITED-STATES; GULF-STREAM
AB Integrating both marine and terrestrial signals from the same sediment core is one of the primary challenges for understanding the role of ocean-atmosphere coupling throughout past climate changes. It is therefore vital to understand how the pollen signal of a given marine record reflects the vegetation changes of the neighboring continent. The comparison between the pollen record of marine core JPC32 (KNR178JPC32) and available terrestrial pollen sequences from eastern North America over the last 12,170 years indicates that the pollen signature off Cape Hatteras gives an integrated image of the regional vegetation encompassing the Pee Dee river, Chesapeake and Delaware hydrographic basins and is reliable in reconstructing the past climate of the adjacent continent. Extremely high quantities of pollen grains included in the marine sediments off Cape Hatteras were transferred from the continent to the sea, at intervals 10,100-8800 cal yr BP, 8300-7500 cal yr BP, 5800-4300 cal yr BP and 2100-730 cal yr BP, during storm events favored by episodes of rapid sea-level rise in the eastern coast of US. In contrast, pollen grains export was reduced during 12,170-10,150 cal yr BP and 4200-2200 cal yr BP, during episodes of intense continental dryness and slow sea level rise episodes or lowstands in the eastern coast of US.
The near absence of reworked pollen grains in core JPC32 contrasts with the high quantity of reworked material in nearby but deeper located marine sites, suggesting that the JPC32 record was not affected by the Deep Western Boundary Current (DWBC) since the end of the Younger Dryas and should be considered a key site for studying past climate changes in the western North Atlantic. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Naughton, F.; Oliveira, D.; Voelker, A.; Abrantes, F.] Portuguese Inst Ocean & Atmosphere IPMA, P-1449006 Lisbon, Portugal.
[Naughton, F.; Oliveira, D.; Abrantes, F.] Univ Algarve, Ctr Marine Sci CCMAR, P-8005139 Faro, Portugal.
[Naughton, F.; Keigwin, L.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Naughton, F.; de Vernal, A.; Voelker, A.] Univ Quebec, GEOTOP Ctr, Montreal, PQ H3C 3P8, Canada.
[Peteet, D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Peteet, D.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Costas, S.] Univ Algarve, CIMA, P-8005139 Faro, Portugal.
[Desprat, S.; Oliveira, D.] Univ Bordeaux, EPHE UMR CNRS EPOC 5805, F-33615 Pessac, France.
RP Naughton, F (reprint author), Portuguese Inst Ocean & Atmosphere IPMA, Ave Brasilia 6, P-1449006 Lisbon, Portugal.
EM filipa.naughton@ipma.pt
RI Desprat, Stephanie/N-7637-2013; Costas, Susana/G-5388-2013; Abrantes,
Fatima /B-5985-2013; Voelker, Antje/C-5427-2012; de Vernal,
Anne/D-5602-2013
OI Naughton, Filipa/0000-0002-3055-9396; Desprat,
Stephanie/0000-0003-4400-679X; Costas, Susana/0000-0002-4005-077X;
Abrantes, Fatima /0000-0002-9110-0212; Voelker,
Antje/0000-0001-6465-6023; de Vernal, Anne/0000-0001-5656-724X
FU Portuguese Foundation for Science and Technology (FCT)
[PTDC/AAC-CLI/100157/2008, SFRH/BPD/36615/2007, SFRH/BPD/96614/2013,
Incentivo/MAR/LA00015/2014]; NSF [OCE-0214144]; FCT project MONA
[PTDC/AAC-AMB/108449/2008]
FX The help and contributions of the following individuals and
organizations are gratefully acknowledged: M.-H. Castera; L. Devaux
(Bordeaux 1 University, EPOC, UMR-CNRS 5805), S. Gomes, T. Rodrigues, E.
Salgueiro and M. Rufino; EPHE-EPOC Bordeaux I University-France,
LNEG-Portugal and the team of the Sintra Library. This research was in
part supported by the Portuguese Foundation for Science and Technology
(FCT) through the project CLIMHOL (PTDC/AAC-CLI/100157/2008) and F.
Naughton's post-doctoral grants (SFRH/BPD/36615/2007 and
SFRH/BPD/96614/2013), CCMAR BCC grant (Incentivo/MAR/LA00015/2014) and
by NSF Grant OCE-0214144 to L D. Keigwin. This research is also a
contribution to FCT project MONA (PTDC/AAC-AMB/108449/2008).
NR 120
TC 1
Z9 1
U1 2
U2 13
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0025-3227
EI 1872-6151
J9 MAR GEOL
JI Mar. Geol.
PD SEP 1
PY 2015
VL 367
BP 118
EP 129
DI 10.1016/j.margeo.2015.06.003
PG 12
WC Geosciences, Multidisciplinary; Oceanography
SC Geology; Oceanography
GA CN4GW
UT WOS:000358389600009
ER
PT J
AU Said, YA
Petropoulos, GP
Srivastava, PK
AF Said, Yahia Abbi
Petropoulos, George P.
Srivastava, Prashant K.
TI Assessing the influence of atmospheric and topographic correction and
inclusion of SWIR bands in burned scars detection from high-resolution
EO imagery: a case study using ASTER
SO NATURAL HAZARDS
LA English
DT Article
DE Burned area mapping; ASTER; Topography; Atmospheric correction; Remote
sensing; Wildfires; Greece
ID SUPPORT VECTOR MACHINES; LANDSAT TM IMAGERY; HYPERION HYPERSPECTRAL
IMAGERY; CLASSIFICATION METHODS; AREA DELINEATION; BOREAL FORESTS;
NATIONAL-PARK; FIRE; VALIDATION; MODIS
AB In the present study, the effect of atmospheric and topographic correction to burned area delineation from Earth Observation (EO) imagery is explored. Furthermore, the potential added value of the inclusion of the shortwave infrared (SWIR) bands for improving retrievals of burned area cartography is investigated. In particular, the capability of ASTER imagery when combined with the maximum likelihood (ML) and the support vector machines (SVMs) classification techniques is examined herein. As a case study, a Mediterranean site on which a fire event occurred in Greece during 2007 and for which post-fire ASTER imagery was available is used. The combination of topographic correction (orthorectification) with the inclusion of the SWIR bands returned the most accurate results in burned area detection. SVMs showed the highest accuracy, showing the most promising potential in delineating the burned areas. The most accurate results for burned scar mapping were obtained from the combined use of SVMs with an orthorectified image and SWIR spectral bands, at least this was the case in our study site. Our results offer a very important contribution to the understanding of the capability of high-resolution imagery such as that from ASTER in burned area estimation. This study also corroborates the usefulness of topographic correction as an image processing step to be incorporated in modelling schemes for delineating burned areas from such data. Findings potentially provide very useful information towards the development of EO-based techniques that aim to operationally provide services related to the estimation of burned area. This is of considerable scientific and practical value to the wider scientific and users' community given the continuation of free access today to observations from space from high-resolution sensors globally.
C1 [Said, Yahia Abbi] Mediterranean Agron Inst Chania, Khania 73100, Crete, Greece.
[Petropoulos, George P.] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 2DB, Dyfed, Wales.
[Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Srivastava, Prashant K.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Srivastava, Prashant K.] Banaras Hindu Univ, Inst Environm & Sustainable Dev, Varanasi 221005, Uttar Pradesh, India.
RP Petropoulos, GP (reprint author), Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 2DB, Dyfed, Wales.
EM george.petropoulos@aber.ac.uk
RI Petropoulos, George/F-2384-2013
OI Petropoulos, George/0000-0003-1442-1423
FU Greek Scholarships Foundation (IKY)
FX George Petropoulos wishes to thank the Greek Scholarships Foundation
(IKY) for the financial support provided to support the implementation
of this study. Authors would also like to thank the anonymous reviewers
for their comments which assisted to improving the originally submitted
manuscript.
NR 57
TC 1
Z9 1
U1 2
U2 10
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0921-030X
EI 1573-0840
J9 NAT HAZARDS
JI Nat. Hazards
PD SEP
PY 2015
VL 78
IS 3
BP 1609
EP 1628
DI 10.1007/s11069-015-1792-9
PG 20
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Water Resources
SC Geology; Meteorology & Atmospheric Sciences; Water Resources
GA CN4OS
UT WOS:000358410300008
ER
PT J
AU Martindale, RC
Strauss, JV
Sperling, EA
Johnson, JE
Van Kranendonk, MJ
Flannery, D
French, K
Lepot, K
Mazumder, R
Rice, MS
Schrag, DP
Summons, R
Walter, M
Abelson, J
Knoll, AH
AF Martindale, Rowan C.
Strauss, Justin V.
Sperling, Erik A.
Johnson, Jena E.
Van Kranendonk, Martin J.
Flannery, David
French, Katherine
Lepot, Kevin
Mazumder, Rajat
Rice, Melissa S.
Schrag, Daniel P.
Summons, Roger
Walter, Malcolm
Abelson, John
Knoll, Andrew H.
TI Sedimentology, chemostratigraphy, and stromatolites of lower
Paleoproterozoic carbonates, Turee Creek Group, Western Australia
SO PRECAMBRIAN RESEARCH
LA English
DT Article
DE Turee Creek Group; Kazput Formation; Kungarra Formation; Great Oxidation
Event; Stromatolite; Lomagundi-Jatuli event
ID SULFIDIC OCEAN TRANSITION; GREAT OXIDATION EVENT; ANIMIKIE BASIN RECORD;
ATMOSPHERIC OXYGEN; HAMERSLEY PROVINCE; SOUTH-AFRICA; QUADRILATERO
FERRIFERO; TRANSVAAL SUPERGROUP; ISOTOPIC EVIDENCE; MINAS SUPERGROUP
AB The ca. 2.45-2.22 Ga Turee Creek Group, Western Australia, contains carbonate-rich horizons that postdate earliest Proterozoic iron formations, bracket both Paleoproterozoic glaciogenic beds and the onset of the Great Oxidation Event (GOE), and predate ca. 2.2-2.05 Ga Lomagundi-Jatuli C-isotopic excursion(s). As such, Turee Creek carbonate strata provide an opportunity to characterize early Paleoproterozoic carbonate sedimentation and carbon cycle dynamics in the context of significant global change. Here, we report on the stratigraphy, sedimentology, petrology, carbon isotope chemostratigraphy, and stromatolite development for carbonate-rich successions within the pre-glacial part of the Kungarra Formation and the postglacial Kazput Formation.
Kungarra carbonate units largely occur as laterally discontinuous beds within a thick, predominantly siliciclastic shelf deposit. While this succession contains thin microbialite horizons, most carbonates consist of patchy calcite overgrowths within a siliciclastic matrix. C-isotopic values show marked variation along a single horizon and even within hand samples, reflecting spatially and temporally variable mixing between dissolved inorganic carbon in seawater and isotopically light inorganic carbon generated via syn- and post-depositional remineralization of organic matter.
In contrast, the Kazput carbonates consist of subtidal stromatolites, grainstones, and micrites deposited on a mixed carbonate-siliciclastic shelf. These carbonates exhibit moderate delta C-13 values of -2 parts per thousand to +1.5 parts per thousand and likely preserve a C-isotopic signature of seawater. Kazput carbonates, thus, provide some of the best available evidence that an interval of unexceptional C-isotopic values separates the Lomagundi-Jatuli C-isotopic excursion(s) from the initiation of the GOE as inferred from multiple sulfur isotopes (loss of mass independent fractionation). The Kazput Formation also contains unusual, m-scale stromatolitic buildups, which are composed of sub-mm laminae and discontinuous, convex upward lenticular precipitates up to a few mm in maximum thickness. Laminae, interpreted as microbial mat layers, contain quartz and clay minerals as well as calcite, whereas precipitate lenses consist of interlocking calcite anhedra, sometimes showing faint mm-scale banding. These cements formed either as infillings of primary voids formed by gas emission within penecontemporaneously lithified mats, or as local seafloor precipitates that formed on, or within, surface mats. It is possible that both mechanisms interacted to form the unique Kazput stromatolites. These microbialites speak to a distinctive interaction between life and environment early in the Paleoproterozoic Era. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Martindale, Rowan C.; Knoll, Andrew H.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Martindale, Rowan C.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA.
[Strauss, Justin V.; Sperling, Erik A.; Schrag, Daniel P.; Knoll, Andrew H.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Johnson, Jena E.; Rice, Melissa S.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Van Kranendonk, Martin J.; Flannery, David; Walter, Malcolm] Univ New South Wales Australia, Australian Ctr Astrobiol, Kensington, NSW 2052, Australia.
[Van Kranendonk, Martin J.] Univ New South Wales Australia, Sch Biol Earth & Environm Sci, Kensington, NSW 2052, Australia.
[Flannery, David; Walter, Malcolm] Univ New South Wales Australia, Sch Biotechnol & Biomol Sci, Kensington, NSW 2052, Australia.
[Flannery, David] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[French, Katherine; Summons, Roger] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Lepot, Kevin] Univ Lille, Lab Oceanol & Geosci, CNRS, UMR8187, F-59655 Villeneuve Dascq, France.
[Mazumder, Rajat] Curtin Univ Sarawak, Fac Sci & Engn, Dept Appl Geol, Miri 98009, Sarawak, Malaysia.
[Rice, Melissa S.] Western Washington Univ, Dept Geol, Bellingham, WA 98225 USA.
[Abelson, John] Agouron Inst, Pasadena, CA 91106 USA.
RP Martindale, RC (reprint author), 1 Univ Stn C1100, Austin, TX 78712 USA.
EM Martindale@jsg.utexas.edu
RI Martindale, Rowan/N-9853-2015; Lepot, Kevin/C-7072-2014
OI Martindale, Rowan/0000-0003-2681-083X; Lepot, Kevin/0000-0003-0556-0405
FU NASA Astrobiological Institute [NNA13AA90A]; NSF; Agouron Institute;
University of New South Wales; Australian Centre for Astrobiology;
Australian Research Council; University of New South Wales [SPF01
PS27782]; NASA Astrobiology Institute [NNA13AA90A]; NSF program on
Frontiers of Earth Science Dynamics
FX We thank R. Shapiro and an anonymous reviewer for constructive comments
on an earlier version of this paper. We thank the Agouron Institute for
funding the 2012 Advanced Geobiology Course to Australia, Henry Goodall
and Guy L'Estrange for logistical support, and Sarah Manley for running
the carbon isotope analyses. R. Martindale thanks Dr. A. H. Knoll and
the NASA Astrobiological Institute Contract NNA13AA90A for providing
postdoctoral funding. J. Strauss and K. French acknowledge NSF graduate
research fellowships for funding support. E. Sperling thanks the Agouron
Institute for an Agouron Postdoctoral Fellowship. D. Flannery was
supported by the University of New South Wales and the Australian Centre
for Astrobiology. M. Walter acknowledges a Professorial Fellowship from
the Australian Research Council. R. Mazumder is grateful to the
University of New South Wales and Agouron Institute for support. M. Van
Kranendonk also acknowledges funding support from the University of New
South Wales grant #SPF01 PS27782. R. Summons and A. Knoll thank the NASA
Astrobiology Institute (Grant #NNA13AA90A). R. Summons was also
supported by the NSF program on Frontiers of Earth Science Dynamics.
NR 87
TC 2
Z9 2
U1 4
U2 33
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0301-9268
EI 1872-7433
J9 PRECAMBRIAN RES
JI Precambrian Res.
PD SEP
PY 2015
VL 266
BP 194
EP 211
DI 10.1016/j.precamres.2015.05.021
PG 18
WC Geosciences, Multidisciplinary
SC Geology
GA CN8PJ
UT WOS:000358702800013
ER
PT J
AU Ries, PA
Janssen, M
AF Ries, Paul A.
Janssen, Michael
TI A large-scale anomaly in Enceladus' microwave emission
SO ICARUS
LA English
DT Article
DE Radio observations; Enceladus; Ices; Satellites, surfaces
ID CASSINI RADAR RADIOMETER; THERMAL EMISSION; 2.2-CM WAVELENGTH; SURFACE;
SATELLITES; IAPETUS; TETHYS; DIONE; RHEA; INERTIA
AB The Cassini spacecraft flew by Enceladus on 6 November 2011, configured to acquire synthetic aperture RADAR imaging of most of the surface with the RADAR instrument. The pass also recorded microwave thermal emission from most of the surface. We report on global patterns of thermal emission at 2.17 cm based on this data set in the context of additional unresolved data both from the ground and from Cassini.
The observed thermal emission is consistent with dielectric constants of pure water or methane ice, but cannot discriminate between the two. The emissivity is similar to those of other icy satellites (approximate to 0.7), consistent with volume scattering. The most intriguing result, however, is an anomaly in the thermal emission of Enceladus' leading hemisphere. Evidence presented here suggests the anomaly is buried at depths on the order of a few meters. This anomaly is located in similar geographic location to anomalies previously detected with the CIRS and ISS instruments on Mimas, Tethys, and Dione (Howett, C.J.A. et al. [2011]. Icarus 216, 221-226; Howett, C.J.A. et al. [2012]. Icarus 221, 1084-1088; Howett, C.J.A. et al. [2014]. Icarus 241, 239-247; Schenk, P. et al. [2011]. Icarus 211, 740-757), but also corresponds with a geological feature on Enceladus' leading terrain (Crow-Willard, E., Pappalardo, R.T. [2011]. Global geological mapping of Enceladus. In: EPSC-DPS Joint Meeting 2011. p. 635). Simple models show that the Crow-Willard and Pappalardo (Crow-Willard, E., Pappalardo, R.T. [2011]. Global geological mapping of Enceladus. In: EPSC-DPS Joint Meeting 2011. p. 635) model is a better fit to the data. Our best-supported hypothesis is that the leading hemisphere smooth terrain is young enough (<75-200 Myr old) that the micrometeorite impact gardening depth is shallower than the electromagnetic skin depth of the observations (approximate to 3-5 m), a picture consistent with ground and space radar measurements, which show no variation at 2 cm, but an increase in albedo in the anomaly region at 13 cm. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Ries, Paul A.; Janssen, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ries, PA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 538-600, Pasadena, CA 91109 USA.
EM paul.a.ries@jpl.nasa.gov; michael.a.janssen@jpl.nasa.gov
FU NASA Postdoctoral Program; NASA; Caltech
FX This research supported by the NASA Postdoctoral Program, administered
by Oak Ridge Associated Universities through a contract with NASA, at
the Jet Propulsion Lab. The Jet Propulsion Lab is operated under
contract by Caltech for NASA. The authors would also like to thank the
anonymous reviewers for their helpful suggestions in improving this
paper.
NR 41
TC 1
Z9 1
U1 1
U2 8
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 1
PY 2015
VL 257
BP 88
EP 102
DI 10.1016/j.icarus.2015.04.030
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN0KA
UT WOS:000358101300006
ER
PT J
AU Grundy, WM
Porter, SB
Benecchi, SD
Roe, HG
Noll, KS
Trujillo, CA
Thirouin, A
Stansberry, JA
Barker, E
Levison, HF
AF Grundy, W. M.
Porter, S. B.
Benecchi, S. D.
Roe, H. G.
Noll, K. S.
Trujillo, C. A.
Thirouin, A.
Stansberry, J. A.
Barker, E.
Levison, H. F.
TI The mutual orbit, mass, and density of the large transneptunian binary
system Varda and Ilmare
SO ICARUS
LA English
DT Article
DE Kuiper belt; Trans-neptunian objects; Satellites, general; Hubble Space
Telescope observations; Astrometry
ID KUIPER-BELT OBJECTS; 42355 TYPHON-ECHIDNA; HERSCHEL-PACS; EVOLUTION;
REGION; TNOS; COOL; SATELLITES; CENTAURS; SALACIA
AB From observations by the Hubble Space Telescope, Keck II Telescope, and Gemini North Telescope, we have determined the mutual orbit of the large transneptunian object (174567) Varda and its satellite Ilmare. These two objects orbit one another in a highly inclined, circular or near-circular orbit with a period of 5.75 days and a semimajor axis of 4810 km. This orbit reveals the system mass to be (2.664 +/- 0.064) x 10(20) kg, slightly greater than the mass of the second most massive main-belt asteroid (4) Vesta. The dynamical mass can in turn be combined with estimates of the surface area of the system from Herschel Space Telescope thermal observations to estimate a bulk density of 1.24(-0.35)(+0.50) g cm(-3). Varda and Ilmare both have colors similar to the combined colors of the system, B-V= 0.886 +/- 0.025 and V-I= 1.156 +/- 0.029. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Grundy, W. M.; Roe, H. G.; Thirouin, A.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Porter, S. B.; Levison, H. F.] Southwest Res Inst, Boulder, CO 80302 USA.
[Benecchi, S. D.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Noll, K. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Trujillo, C. A.] Gemini Observ, Hilo, HI 96720 USA.
[Stansberry, J. A.; Barker, E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Grundy, WM (reprint author), Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA.
EM W.Grundy@lowell.edu
FU NASA through grants from the Space Telescope Science Institute (STScI)
[NAS 5-26555]; W.M. Keck Foundation; NASA Keck PI Data Awards; NSF
Planetary Astronomy Grant [AST-1109872]
FX This work is based in part on NASA/ESA Hubble Space Telescope programs
11113 and 12237. Support for these programs was provided by NASA through
grants from the Space Telescope Science Institute (STScI), operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA Contract NAS 5-26555. We are especially grateful to Tony Roman at
STScI for his efficiency in scheduling HST follow-up observations in
program 12237.; Additional data 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 and made possible by the generous financial support of the W.M.
Keck Foundation. These data were obtained from telescope time allocated
to NASA through the agency's scientific partnership with the California
Institute of Technology and the University of California and their
acquisition was supported by NASA Keck PI Data Awards, administered by
the NASA Exoplanet Science Institute.; This work was supported in part
by NSF Planetary Astronomy Grant AST-1109872. The authors wish to
recognize and acknowledge the significant cultural role and reverence of
the summit of Mauna Kea within the indigenous Hawaiian community. We are
grateful to have been able to observe from this mountain. This
manuscript benefited from reviews by D. Ragozzine and an anonymous
reviewer. We thank them for the time and effort they contributed to
improving the paper. Finally, we thank the free and open source software
communities for empowering us with key tools used to complete this
project, notably Linux, the GNU tools, LibreOffice, MariaDB, Evolution,
Python, the Astronomy User's Library, and FVWM.
NR 61
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U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 1
PY 2015
VL 257
BP 130
EP 138
DI 10.1016/j.icarus.2015.04.036
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN0KA
UT WOS:000358101300010
ER
PT J
AU McFadden, LA
Skillman, DR
Memarsadeghi, N
Li, JY
Joy, SP
Polanskey, CA
Rayman, MD
Sykes, MV
Tricarico, P
Palmer, E
O'Brien, DP
Mottola, S
Carsenty, U
Mutchler, M
McLean, B
Schroder, SE
Mastrodemos, N
Schiff, C
Keller, HU
Nathues, A
Gutierrez-Marques, P
Raymond, CA
Russell, CT
AF McFadden, Lucy A.
Skillman, David R.
Memarsadeghi, Nargess
Li, Jian-Yang
Joy, S. P.
Polanskey, C. A.
Rayman, Marc D.
Sykes, Mark V.
Tricarico, Pasquale
Palmer, Eric
O'Brien, David P.
Mottola, Stefano
Carsenty, Uri
Mutchler, Max
McLean, Brian
Schroeder, Stefan E.
Mastrodemos, Nicolas
Schiff, Conrad
Keller, H. Uwe
Nathues, Andreas
Gutierrez-Marques, Pablo
Raymond, C. A.
Russell, C. T.
TI Vesta's missing moons: Comprehensive search for natural satellites of
Vesta by the Dawn spacecraft
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids, dynamics; Satellites of asteroids
ID ASTEROID 4 VESTA; FRAMING CAMERA; ORIGIN; BELT; CALIBRATION; METEORITES;
EVOLUTION; DISCOVERY; CATALOG; FAMILY
AB Earth-bound searches for natural satellites of 4 Vesta have been reported since 1987. With use of technological advances and observing capability has come a reduction in the detectable size of a possible satellite. The Dawn mission brought a small camera close to Vesta itself. In our search, which was carried out with a comprehensive data acquisition strategy and by experienced searchers, we find no satellites to a detection limit as small as 3-m radius. Various observation and analysis strategies are discussed in detail. It is now time to factor the null result of this search into the context of satellite formation among other main belt asteroids and to conduct dynamical modeling to explore the suspected forces contributing to the absence of satellites at Vesta today. Published by Elsevier Inc.
C1 [McFadden, Lucy A.; Skillman, David R.; Memarsadeghi, Nargess; Schiff, Conrad] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Li, Jian-Yang; Sykes, Mark V.; Tricarico, Pasquale; Palmer, Eric; O'Brien, David P.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Joy, S. P.; Russell, C. T.] Univ Calif Los Angeles, IGPP, Los Angeles, CA 90095 USA.
[Polanskey, C. A.; Rayman, Marc D.; Mastrodemos, Nicolas; Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mottola, Stefano; Carsenty, Uri; Schroeder, Stefan E.] Inst Planetary Res, DLR German Aerosp Ctr, Berlin, Germany.
[Mutchler, Max; McLean, Brian] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Keller, H. Uwe] Tech Univ Carolo Wilhelmina Braunschweig, IGEP, Braunschweig, Germany.
[Nathues, Andreas; Gutierrez-Marques, Pablo] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
RP McFadden, LA (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Code 693,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM lucy.mcfadden@nasa.gov
RI Schroder, Stefan/D-9709-2013;
OI Schroder, Stefan/0000-0003-0323-8324; McFadden, Lucy/0000-0002-0537-9975
FU Dawn mission through NASA's Discovery Program; NASA's Dawn at Vesta
Participating Scientist Program [NNX10AR56G, NNX13AB82G]; NASA
[NNM05AA86C]; Max Planck Society - Germany; German Space Agency, DLR
FX We thank Herbert Raab for working with us to modify Astrometrica so that
asteroids could be projected into the Dawn spacecraft's frame of
reference. The Dawn Flight Team made the observations possible and we
thank them for their superior driving and operations implementation.
This work was supported by the Dawn mission through NASA's Discovery
Program, NASA's Dawn at Vesta Participating Scientist Program through
Grants NNX10AR56G to University of Maryland at College Park and
NNX13AB82G to Planetary Science Institute. Part of this work was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA to UCLA NASA contract number,
NNM05AA86C. The Framing Camera project is financially supported by the
Max Planck Society - Germany and the German Space Agency, DLR.
NR 48
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U2 2
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 1
PY 2015
VL 257
BP 207
EP 216
DI 10.1016/j.icarus.2015.04.038
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN0KA
UT WOS:000358101300015
ER
PT J
AU Vixie, G
Barnes, JW
Jackson, B
Rodriguez, S
Le Mouelic, S
Sotin, C
MacKenzie, S
Wilson, P
AF Vixie, Graham
Barnes, Jason W.
Jackson, Brian
Rodriguez, Sebastien
Le Mouelic, Stephane
Sotin, Christophe
MacKenzie, Shannon
Wilson, Paul
TI Possible temperate lakes on Titan
SO ICARUS
LA English
DT Article
DE Titan, hydrology; Titan, atmosphere; Titan, surface; Radiative transfer
ID CASSINI VIMS; MIDLATITUDE CLOUDS; HYDROCARBON LAKES; ONTARIO LACUS;
LANDING SITE; DUNE FIELDS; SURFACE; RADAR; ATMOSPHERE; AEROSOLS
AB We analyze southern mid-latitude albedo-dark features on Titan observed by Cassini's Visual and Infrared Mapping Spectrometer (VIMS). In exploring the nature of these features we consider their morphology, albedo, and specular reflectivity. We suggest that they represent candidates for potential temperate lakes. The presence of lakes at the mid-latitudes would indicate that surface liquid can accumulate and remain stable away from Titan's poles. Candidate lakes were identified by looking for possible shorelines with "lacustrine morphology. Then, we applied an atmospheric correction that empirically solved for their surface albedo. Finally, we looked for a specular reflection of the sky in the identified candidates. Using this prescription, we find two candidates that remain as potential temperature lakes. If candidate features do represent temperate lakes on Titan, they have implications for formation mechanisms such as clouds and rainfall or, in low elevation areas, percolation and subsurface flow. Clouds were observed near candidate lake locations on the T66 flyby and this latitude band showed many clouds during southern summer. Our techniques can be applied to areas of Titan that lack RADAR coverage to search for mid- and low-latitude lakes in the future. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Vixie, Graham; Barnes, Jason W.; MacKenzie, Shannon] Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
[Jackson, Brian] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Rodriguez, Sebastien] Univ Paris 07, Lab AIM, CNRS, CEA Saclay,DSM,IRFU,SAp, Gif Sur Yvette, France.
[Le Mouelic, Stephane] Univ Nantes, LPGN, CNRS, UMR6112, Nantes, France.
[Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wilson, Paul] Energyneering Solut, Sisters, OR 97759 USA.
RP Vixie, G (reprint author), Univ Idaho, Dept Phys, 875 Perimeter Dr,MS0903, Moscow, ID 83844 USA.
EM gvixie@vandals.uidaho.edu
RI Barnes, Jason/B-1284-2009; Rodriguez, Sebastien/H-5902-2016
OI Barnes, Jason/0000-0002-7755-3530; Rodriguez,
Sebastien/0000-0003-1219-0641
FU NASA Outer Planets Research Program [NNX09AP34G]
FX The author acknowledges funding by Grant #NNX09AP34G to JWB from the
NASA Outer Planets Research Program.
NR 53
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 1
PY 2015
VL 257
BP 313
EP 323
DI 10.1016/j.icarus.2015.05.009
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN0KA
UT WOS:000358101300024
ER
PT J
AU Rodriguez, JAP
Platz, T
Gulick, V
Baker, VR
Fairen, AG
Kargel, J
Yan, JG
Miyamoto, H
Glines, N
AF Rodriguez, J. Alexis P.
Platz, Thomas
Gulick, Virginia
Baker, Victor R.
Fairen, Alberto G.
Kargel, Jeffrey
Yan, Jianguo
Miyamoto, Hideaki
Glines, Natalie
TI Did the martian outflow channels mostly form during the Amazonian
Period?
SO ICARUS
LA English
DT Article
DE Terrestrial planets; Mars; Surface; Hydrology
ID VALLES-MARINERIS; NORTHERN PLAINS; HYDROLOGICAL CYCLE; ARES VALLIS;
MARS; CRATER; GLACIATION; EVOLUTION; SURFACE; ORIGIN
AB Simud, Tiu, and Ares Valles comprise some of the largest outflow channels on Mars. Their excavation has been attributed variously to (or a combination of) erosion by catastrophic floods, glaciers, and debris flows. Numerous investigations indicate that they formed largely during the Late Hesperian (3.61-3.37 Ga). However, these studies mostly equate the ages of the outflow channel floors to those of the flows that generated mesoscale (several hundred meters to a few kilometers) bedforms within them. To improve the statistical accuracy in the age determinations of these flow events, we have used recently acquired high-resolution image and topographic data to map and date portions of Simud, Tiu and Ares Valles, which are extensively marked by these bedforms. Our results, which remove the statistical effects of older and younger outflow channel floor surfaces on the generation of modeled ages, reveal evidence for major outflow channel discharges occurring during the Early (3.37-1.23 Ga) and Middle (1.23-0.328 Ga) Amazonian, with activity significantly peaking during the Middle Amazonian stages. We also find that during the documented stages of Middle Amazonian discharges, the floor of Tiu Valles underwent widespread collapse, resulting in chaotic terrain formation. In addition, we present evidence showing that following the outflow channel discharges, collapse within northern Simud Valles generated another chaotic terrain. This younger chaos region likely represents the latest stage of large-scale outflow channel resurfacing within the study area. Our findings imply that in southern circum-Chryse the martian hydrosphere experienced large-scale drainage during the Amazonian, which likely led to periodic inundation and sedimentation within the northern plains. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Rodriguez, J. Alexis P.; Gulick, Virginia; Glines, Natalie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rodriguez, J. Alexis P.; Platz, Thomas] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Platz, Thomas] Free Univ Berlin, Inst Geol Sci, Planetary Sci & Remote Sensing, D-12249 Berlin, Germany.
[Gulick, Virginia; Glines, Natalie] SETI Inst, Mountain View, CA 94043 USA.
[Baker, Victor R.; Kargel, Jeffrey] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
[Fairen, Alberto G.] Ctr Astrobiol, Madrid 28850, Spain.
[Fairen, Alberto G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Yan, Jianguo] State Key Lab Informat Engn Surveying Mapping & R, Wuhan 430070, Peoples R China.
[Miyamoto, Hideaki] Univ Tokyo, Univ Museum, Tokyo 1130033, Japan.
RP Rodriguez, JAP (reprint author), Planetary Sci Inst, 1700 East Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA.
RI Platz, Thomas/F-7539-2013; Miyamoto, Hideaki/B-9666-2008
OI Platz, Thomas/0000-0002-1253-2034;
FU NASA; MRO HiRISE Co-Investigator funds; DFG [PL613/2-1]; Helmholtz
Association; European Research Council under the European Union's
Seventh Framework Programme, ERC [307496]; KAKENHI [23340126]
FX We are grateful to N.G. Barlow and G. Komatsu for their insightful
reviews, which have significantly improved this manuscript. Funding
provided by NASA's NPP program to J. Alexis P. Rodriguez and by MRO
HiRISE Co-Investigator funds to V.C. Gulick. T. Platz was supported by a
DFG Grant (PL613/2-1) and the Helmholtz Association through the research
alliance "Planetary Evolution and Life". A.G. Fairen was supported by
the European Research Council under the European Union's Seventh
Framework Programme (FP7/20072013), ERC Grant Agreement No. 307496.
HiRISE images were analyzed using HiView developed by the Lunar and
Planetary Laboratory at the University of Arizona. The participation of
Hideaki Miyamoto was supported by Grant KAKENHI 23340126.
NR 67
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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 SEP 1
PY 2015
VL 257
BP 387
EP 395
DI 10.1016/j.icarus.2015.04.024
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CN0KA
UT WOS:000358101300030
ER
PT J
AU Righter, K
AF Righter, Kevin
TI Magma Ocean Depth and Oxygen Fugacity in the Early Earth-Implications
for Biochemistry
SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES
LA English
DT Article
DE Core; Siderophile; Sulfur; Nitrogen; Carbon; Hydrogen; Redox
ID CORE FORMATION; HIGH-PRESSURE; NITROGEN SOLUBILITY; TERRESTRIAL PLANET;
REDOX SYSTEMATICS; OXIDATION-STATE; SILICATE; METAL; MANTLE; IRON
AB A large class of elements, referred to as the siderophile (iron-loving) elements, in the Earth's mantle can be explained by an early deep magma ocean on the early Earth in which the mantle equilibrated with metallic liquid (core liquid). This stage would have affected the distribution of some of the classic volatile elements that are also essential ingredients for life and biochemistry - H, C, S, and N. Estimates are made of the H, C, S, and N contents of Earth's early mantle after core formation, considering the effects of variable temperature, pressure, oxygen fugacity, and composition on their partitioning. Assessment is made of whether additional, exogenous, sources are required to explain the observed mantle concentrations, and areas are identified where additional data and experimentation would lead to an improved understanding of this phase of Earth's history.
C1 NASA Johnson Space Ctr, Houston, TX 77058 USA.
RP Righter, K (reprint author), NASA Johnson Space Ctr, Mailcode XI2,2101 NASA Pkwy, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
NR 38
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U1 6
U2 13
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-6149
EI 1573-0875
J9 ORIGINS LIFE EVOL B
JI Orig. Life Evol. Biosph.
PD SEP
PY 2015
VL 45
IS 3
BP 361
EP 366
DI 10.1007/s11084-015-9445-2
PG 6
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA CN3ZG
UT WOS:000358366700010
PM 26037825
ER
PT J
AU Cataldo, G
Moseley, SH
Wollack, EJ
AF Cataldo, Giuseppe
Moseley, Samuel H.
Wollack, Edward J.
TI A four-pole power-combiner design for far-infrared and submillimeter
spectroscopy
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Far-infrared; Spectroscopy; Stigmatic points; Design optimization; Space
systems
ID SPECTROMETER; SPEC
AB The far-infrared and submillimeter portions of the electromagnetic spectrum provide a unique view of the astrophysical processes present in the early universe. Micro-Spec (mu-Spec), a high-efficiency direct-detection spectrometer concept working in the 450-1000-mu m wavelength range, will enable a wide range of spaceflight missions that would otherwise be challenging due to the large size of current instruments and the required spectral resolution and sensitivity. This paper focuses on the mu-Spec two-dimensional multimode region, where the light of different wavelengths diffracts and converges onto a set of detectors. A two-step optimization process is used to generate geometrical configurations given specific requirements on spectrometer size, operating spectral range, and performance. The canonically employed focal-plane constraints for the power combiner were removed to probe the design space in its entirety. A new four-stigmatic-point optical design solution is identified and explored for use in far-infrared and submillimeter spectroscopy. (C) 2015 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Cataldo, Giuseppe; Moseley, Samuel H.; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cataldo, Giuseppe] MIT, Cambridge, MA 02139 USA.
RP Cataldo, G (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Giuseppe.Cataldo@nasa.gov
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
FU NASA ROSES/APRA program; Massachusetts Institute of Technology "Arthur
Gelb" fellowship
FX G.C. would like to thank Prof. Jeffrey A. Hoffman, thesis advisor, for
helpful revisions and discussions. The authors gratefully acknowledge
the financial support received from the NASA ROSES/APRA program and the
Massachusetts Institute of Technology "Arthur Gelb" fellowship.
NR 27
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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 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2015
VL 114
BP 54
EP 59
DI 10.1016/j.actaastro.2015.04.002
PG 6
WC Engineering, Aerospace
SC Engineering
GA CM7VX
UT WOS:000357905700005
ER
PT J
AU Menzies, T
Pasareanu, C
AF Menzies, Tim
Pasareanu, Corina
TI Guest editorial: special multi-issue on selected topics in Automated
Software Engineering
SO AUTOMATED SOFTWARE ENGINEERING
LA English
DT Editorial Material
C1 [Menzies, Tim] N Carolina State Univ, Dept Comp Sci, Raleigh, NC 27695 USA.
[Pasareanu, Corina] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA.
[Pasareanu, Corina] NASA Ames, Pittsburgh, PA USA.
RP Menzies, T (reprint author), N Carolina State Univ, Dept Comp Sci, Raleigh, NC 27695 USA.
EM tim.menzies@gmail.com; corina.s.pasareanu@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0928-8910
EI 1573-7535
J9 AUTOMAT SOFTW ENG
JI Automat. Softw. Eng.
PD SEP
PY 2015
VL 22
IS 3
SI SI
BP 289
EP 290
DI 10.1007/s10515-015-0180-8
PG 2
WC Computer Science, Software Engineering
SC Computer Science
GA CM4JQ
UT WOS:000357651200001
ER
PT J
AU Leone, FA
AF Leone, Frank A., Jr.
TI Deformation gradient tensor decomposition for representing matrix cracks
in fiber-reinforced materials
SO COMPOSITES PART A-APPLIED SCIENCE AND MANUFACTURING
LA English
DT Article
DE Damage mechanics; Finite element analysis (FEA); Polymer-matrix
composites
ID CONSTITUTIVE MODEL; DAMAGE MODEL; COMPOSITES; DELAMINATION; SIMULATION;
FAILURE
AB A new method is presented for the representation of matrix cracks in continuum damage mechanics (CDM) models for fiber-reinforced materials. The method is based on the additive decomposition of the deformation gradient tensor into 'crack' and 'bulk material' components, analogous to the additive strain decomposition of the smeared-crack approach. The potential improvements to the accuracy of CDM models that utilize the presented method are demonstrated for a single element subjected to simple shear deformation and for a unidirectional open-hole tension specimen. The presented method avoids load transfer across matrix cracks and eliminates the prediction of spurious secondary failure modes that occurs when conventional strain-based CDM models are used in geometrically nonlinear finite element analyses involving large shear deformations. Published by Elsevier Ltd.
C1 NASA Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
RP Leone, FA (reprint author), NASA Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
EM frank.a.leone@nasa.gov
NR 20
TC 0
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U1 2
U2 5
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1359-835X
EI 1878-5840
J9 COMPOS PART A-APPL S
JI Compos. Pt. A-Appl. Sci. Manuf.
PD SEP
PY 2015
VL 76
BP 334
EP 341
DI 10.1016/j.compositesa.2015.06.014
PG 8
WC Engineering, Manufacturing; Materials Science, Composites
SC Engineering; Materials Science
GA CN0IC
UT WOS:000358096300038
ER
PT J
AU Jackson, WA
Bohlke, JK
Andraski, BJ
Fahlquist, L
Bexfield, L
Eckardt, FD
Gates, JB
Davila, AF
McKay, CP
Rao, B
Sevanthi, R
Rajagopalan, S
Estrada, N
Sturchio, N
Hatzinger, PB
Anderson, TA
Orris, G
Betancourt, J
Stonestrom, D
Latorre, C
Li, YH
Harvey, GJ
AF Jackson, W. Andrew
Boehlke, J. K.
Andraski, Brian J.
Fahlquist, Lynne
Bexfield, Laura
Eckardt, Frank D.
Gates, John B.
Davila, Alfonso F.
McKay, Christopher P.
Rao, Balaji
Sevanthi, Ritesh
Rajagopalan, Srinath
Estrada, Nubia
Sturchio, Neil
Hatzinger, Paul B.
Anderson, Todd A.
Orris, Greta
Betancourt, Julio
Stonestrom, David
Latorre, Claudio
Li, Yanhe
Harvey, Gregory J.
TI Global patterns and environmental controls of perchlorate and nitrate
co-occurrence in arid and semi-arid environments
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID OXYGEN ISOTOPIC COMPOSITIONS; NATURAL PERCHLORATE; UNITED-STATES;
NORTHWESTERN CHINA; FRESH-WATER; HIGH-PLAINS; DESERT; GROUNDWATER; SOIL;
REDUCTION
AB Natural perchlorate (ClO4) is of increasing interest due to its wide-spread occurrence on Earth and Mars, yet little information exists on the relative abundance of ClO4- compared to other major anions, its stability, or long-term variations in production that may impact the observed distributions. Our objectives were to evaluate the occurrence and fate of ClO4- in groundwater and soils/caliche in arid and semi-arid environments (southwestern United States, southern Africa, United Arab Emirates, China, Antarctica, and Chile) and the relationship of ClO4 to the more well-studied atmospherically deposited anions NO3- and Cl- as a means to understand the prevalent processes that affect the accumulation of these species over various time scales. ClO4- is globally distributed in soil and groundwater in arid and semi-arid regions on Earth at concentrations ranging from 10(-1) to 10(6) mu g/kg. Generally, the ClO4- concentration in these regions increases with aridity index, but also depends on the duration of arid conditions. In many arid and semi-arid areas, NO3- and ClO4- co-occur at molar ratios (NO3-/ClO4-) that vary between similar to 10(4) and 10(5). We hypothesize that atmospheric deposition ratios are largely preserved in hyper-arid areas that support little or no biological activity (e.g. plants or bacteria), but can be altered in areas with more active biological processes including N-2 fixation, N mineralization, nitrification, denitrification, and microbial ClO4- reduction, as indicated in part by NO3- isotope data. In contrast, much larger ranges of Cl-/ClO4- and Cl-/NO3- ratios indicate Cl- varies independently from both ClO4- and NO3-. The general lack of correlation between Cl- and ClO4- or NO3- implies that Cl- is not a good indicator of co-deposition and should be used with care when interpreting oxyanion cycling in arid systems. The Atacama Desert appears to be unique compared to all other terrestrial locations having a NO3-/ClO4- molar ratio similar to 10(3). The relative enrichment in ClO4- compared to Cl- or NO3- and unique isotopic composition of Atacama ClO4- may reflect either additional in-situ production mechanism(s) or higher relative atmospheric production rates in that specific region or in the geological past. Elevated concentrations of ClO4- reported on the surface of Mars, and its enrichment with respect to Cl- and NO3-, could reveal important clues regarding the climatic, hydrologic, and potentially biologic evolution of that planet. Given the highly conserved ratio of NO3-/ClO4- in non-biologically active areas on Earth, it may be possible to use alterations of this ratio as a biomarker on Mars and for interpreting major anion cycles and processes on both Mars and Earth, particularly with respect to the less-conserved NO3- pool terrestrially. (C) 2015 Elsevier Ltd.
All rights reserved.
C1 [Jackson, W. Andrew; Rao, Balaji; Sevanthi, Ritesh; Estrada, Nubia; Anderson, Todd A.] Texas Tech Univ, Lubbock, TX 79409 USA.
[Boehlke, J. K.; Betancourt, Julio] US Geol Survey, Natl Ctr 431, Reston, VA 20192 USA.
[Andraski, Brian J.] US Geol Survey, Carson City, NV 89701 USA.
[Fahlquist, Lynne] US Geol Survey, Austin, TX 78754 USA.
[Bexfield, Laura] US Geol Survey, Albuquerque, NM 87109 USA.
[Eckardt, Frank D.] Univ Cape Town, Dept Environm & Geog Sci, ZA-7701 Rondebosch, South Africa.
[Gates, John B.] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA.
[Davila, Alfonso F.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rajagopalan, Srinath] SSN Coll Engn, Dept Civil Engn, Kalavakkam 603110, India.
[Sturchio, Neil] Univ Delaware, Dept Geol Sci, Newark, DE 19716 USA.
[Hatzinger, Paul B.] CB&I Fed Serv, Lawrenceville, NJ 08648 USA.
[Orris, Greta] US Geol Survey, Tucson, AZ USA.
[Stonestrom, David] US Geol Survey, Menlo Pk, CA 94025 USA.
[Latorre, Claudio] Inst Ecol & Biodivers IEB, Santiago, Chile.
[Latorre, Claudio] Pontificia Univ Catolica Chile, Dept Ecol, Santiago, Chile.
[Li, Yanhe] Chinese Acad Geol Sci, Inst Mineral Resources, Key Lab Metallogeny & Mineral Assessment, Beijing 100037, Peoples R China.
[Harvey, Gregory J.] USAFSAM OEC, Wright Patterson AFB, OH 45433 USA.
RP Jackson, WA (reprint author), Texas Tech Univ, Lubbock, TX 79409 USA.
EM andrew.jackson@ttu.edu
RI Jackson, William/B-8999-2009; Eckardt, Frank/N-3682-2015; Latorre
Hidalgo, Claudio/E-6805-2012;
OI Eckardt, Frank/0000-0003-0200-7110; Latorre Hidalgo,
Claudio/0000-0003-4708-7599; Stonestrom, David/0000-0001-7883-3385;
Sevanthi, Ritesh/0000-0002-7651-3553; Anderson, Todd/0000-0001-8176-6339
FU Strategic Environmental Research and Development Program (SERDP) of U.S.
Department of Defense [ER-1435]; U.S. Geological Survey Toxic Substances
Hydrology Program; National Research Program; Groundwater Resources
Program; National Water Quality Assessment Program; U.S. Antarctic
Research Program[NSF]; Abu Dhabi Emirate National Drilling Company;
[ICM P05-002]; [PFB-23]
FX This work was supported by the Strategic Environmental Research and
Development Program (SERDP Project ER-1435) of the U.S. Department of
Defense; the U.S. Geological Survey Toxic Substances Hydrology Program,
National Research Program, Groundwater Resources Program, and National
Water Quality Assessment Program; the U.S. Antarctic Research
Program[NSF]; and the Abu Dhabi Emirate National Drilling Company. CL
acknowledges additional support from grants ICM P05-002 and PFB-23 to
the IEB. We are also grateful to SQM for allowing access to a nitrate
mine. We thank Dr. Peter McMahon, Dr. Hans Eggenkamp, and anonymous
reviewers for insightful comments and suggestions on the manuscript. We
thank J. Hannon and S. Mroczkowski for assistance with nitrate isotopic
analyses. Any use of trade, product, or firm names is for descriptive
purposes only and does not imply endorsement by the U.S. Government.
NR 64
TC 14
Z9 14
U1 8
U2 51
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD SEP 1
PY 2015
VL 164
BP 502
EP 522
DI 10.1016/j.gca.2015.05.016
PG 21
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CM9IM
UT WOS:000358021900030
ER
PT J
AU Chen, Y
Liu, Y
Guan, YB
Eiler, JM
Ma, C
Rossman, GR
Taylor, LA
AF Chen, Yang
Liu, Yang
Guan, Yunbin
Eiler, John M.
Ma, Chi
Rossman, George R.
Taylor, Lawrence A.
TI Evidence in Tissint for recent subsurface water on Mars
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mars; Amazonian; water activity; Tissint meteorite; impact melt
ID MARTIAN SOIL COMPONENT; MELT INCLUSIONS; AQUEOUS ALTERATION; HYDROGEN
ISOTOPES; METEORITE; SHERGOTTITE; ABUNDANCES; MANTLE; ATMOSPHERE;
MINERALS
AB We report unambiguous chemical evidence for subsurface water activity in the martian crust at <600 Ma based on the data from Tissint, a fresh martian meteorite fall with minimal terrestrial weathering. The impact-melt pockets in Tissint contain abundant volatiles (H2O, CO2, F, and Cl), and their concentrations are positively correlated with each other. Higher H2O concentrations also accompany higher deuterium contents. These correlations suggest mixing between two volatile sources. The first source is H2O in the precursor basalt inherited from martian magma. Magmatic H2O in the basalt had low deuterium concentration and was likely stored in the nominally anhydrous minerals. This source contributed little CO2 or halogens to the impact melts. The second source is inferred to be aqueous-alteration products introduced to the basalt by water activity after the basalt erupted. These alteration materials contributed more volatiles to the impact melts than the magmatic source, and had high deuterium abundance, reflecting isotope equilibrium with recent martian atmosphere. The water activities occurred beneath the martian surface after 600 Ma (crystallization age), but before 1 Ma (ejection age). The chemical and isotopic signatures of the alteration products in Tissint resemble previously known martian samples associated with old water activities on Mars, which can be traced back to similar to 4.2 billion years ago (e.g., the mudstone at Gale Crater). This similarity in chemistry and the wide age-span indicate that such water activities were common on Mars throughout its history, which had the potential to form habitable environment. However, the rarity of the volatile-rich zone in Tissint suggests that Martian crustal aqueous processes, where they have occurred are generally limited in their extent of water-rock reaction. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Chen, Yang; Liu, Yang] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Guan, Yunbin; Eiler, John M.; Ma, Chi; Rossman, George R.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Taylor, Lawrence A.] Univ Tennessee, Dept Earth & Planetary Sci, Planetary Geosci Inst, Knoxville, TN 37996 USA.
RP Chen, Y (reprint author), Jet Prop Lab, M-S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Yang.Chen@jpl.nasa.gov
OI Rossman, George/0000-0002-4571-6884; Chen, Yang/0000-0003-4729-3499
FU Jet Propulsion Laboratory; NASA [NNN13D465T, NNX11AG58G]; NSF
[EAR-1322082, EAR-0318518, DMR-00800065]; Gordon and Betty Moore
Foundation
FX Authors Y.C. and Y.L. are supported by the Jet Propulsion Laboratory,
which is managed by the California Institute of Technology (Caltech)
under a contract with NASA. We thank Chris Webster for his comments on
an earlier draft. We thank Tamsin Mather, Tomohiro Usui, and one
anonymous reviewer for their constructive comments. Y.L. and L.A.T.
acknowledge NASA Cosmochemistry grants NNN13D465T and NNX11AG58G,
respectively. Funding from NSF grant EAR-1322082 is acknowledged by
G.R.R. The EPMA and SEM were performed at the Caltech Geological and
Planetary Science Division Analytical Facility, which is supported in
part by NSF grants EAR-0318518 and DMR-00800065. Analysis by SIMS was
done at the Caltech Microanalysis Center that is partially supported by
the Gordon and Betty Moore Foundation.
NR 44
TC 9
Z9 9
U1 7
U2 45
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
EI 1385-013X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD SEP 1
PY 2015
VL 425
BP 55
EP 63
DI 10.1016/j.epsl.2015.05.004
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA CM5UU
UT WOS:000357755300006
ER
PT J
AU Casner, SM
Schooler, JW
AF Casner, Stephen M.
Schooler, Jonathan W.
TI Vigilance impossible: Diligence, distraction, and daydreaming all lead
to failures in a practical monitoring task
SO CONSCIOUSNESS AND COGNITION
LA English
DT Article
DE Vigilance; Monitoring; Mind wandering; Task-unrelated thought;
Distraction; Divided attention; Cockpit; Airline pilots
ID SUSTAINED ATTENTION; MIND; PERFORMANCE
AB In laboratory studies of vigilance, participants watch for unusual events in a "sit and stare" fashion as their performance typically declines over time. But watch keepers in practical settings seldom approach monitoring in such simplistic ways and controlled environments. We observed airline pilots performing routine monitoring duties in the cockpit. Unlike laboratory studies, pilots' monitoring did not deteriorate amidst prolonged vigils. Monitoring was frequently interrupted by other pop-up tasks and misses followed. However, when free from these distractions, pilots reported copious mind wandering. Pilots often confined their mind wandering to times in which their monitoring performance would not conspicuously suffer. But when no convenient times were available, pilots mind wandered anyway and misses ensued. Real-world monitors may be caught between a continuous vigilance approach that is doomed to fail, a dynamic environment that cannot be fully controlled, and what may be an irresistible urge to let one's thoughts drift.
C1 [Casner, Stephen M.] NASA, Moffett Field, CA 94035 USA.
[Schooler, Jonathan W.] Univ Calif Santa Barbara, Dept Psychol & Brain Sci, Santa Barbara, CA 93106 USA.
RP Casner, SM (reprint author), NASA, Mail Stop 262-4, Moffett Field, CA 94035 USA.
EM stephen.casner@nasa.gov; jonathan.schooler@psych.ucsb.edu
FU National Aeronautics and Space Administration under the agency's
Aviation Safety Program
FX This work was internally funded by the National Aeronautics and Space
Administration under the agency's Aviation Safety Program. Kevin Koehn
assisted in analyzing the video data. Ed Hutchins provided valuable
insights.
NR 36
TC 4
Z9 4
U1 1
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1053-8100
EI 1090-2376
J9 CONSCIOUS COGN
JI Conscious. Cogn.
PD SEP
PY 2015
VL 35
BP 33
EP 41
DI 10.1016/j.concog.2015.04.019
PG 9
WC Psychology, Experimental
SC Psychology
GA CL5LD
UT WOS:000357000500004
PM 25966369
ER
PT J
AU Dlugach, JM
Mishchenko, MI
AF Dlugach, Janna M.
Mishchenko, Michael I.
TI Scattering properties of heterogeneous mineral particles with absorbing
inclusions
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Maxwell equations; Electromagnetic scattering; Superposition T-matrix
method; Heterogeneous particles
ID RADIATIVE PROPERTIES; T-MATRIX; SOOT AEROSOLS; COMPLEX SOOT
AB We analyze the results of numerically exact computer modeling of scattering and absorption properties of randomly oriented polydisperse heterogeneous particles obtained by placing microscopic absorbing grains randomly on the surfaces of much larger spherical mineral hosts or by imbedding them randomly inside the hosts. These computations are paralleled by those for heterogeneous particles obtained by fully encapsulating fractal-like absorbing clusters in the mineral hosts. All computations are performed using the superposition T-matrix method. In the case of randomly distributed inclusions, the results are compared with the outcome of Lorenz-Mie computations for an external mixture of the mineral hosts and absorbing grains. We conclude that internal aggregation can affect strongly both the integral radiometric and differential scattering characteristics of the heterogeneous particle mixtures. Published by Elsevier Ltd.
C1 [Dlugach, Janna M.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine.
[Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM michael.i.mishchenko@nasa.gov
FU National Academy of Sciences of Ukraine under the Main Astronomical
Observatory GRAPE/GPU/GRID Computing Cluster Project; NASA Radiation
Sciences Program; NASA ACE Project
FX We thank Alexandra Ivanova for help with Fig. 1. JMD acknowledges
support from the National Academy of Sciences of Ukraine under the Main
Astronomical Observatory GRAPE/GPU/GRID Computing Cluster Project. She
also thanks the organizers of the LIP 2014 conference for providing full
financial support. MIM was supported by the NASA Radiation Sciences
Program and the NASA ACE Project managed by Hal Maring as well as by the
NASA Remote Sensing Theory Program managed by Lucia Tsaoussi.
NR 17
TC 5
Z9 5
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD SEP
PY 2015
VL 162
SI SI
BP 89
EP 94
DI 10.1016/j.jqsrt.2015.01.012
PG 6
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA CM2WU
UT WOS:000357543800009
ER
PT J
AU Lock, JA
Mishchenko, MI
AF Lock, James A.
Mishchenko, Michael I.
TI A persistent feature of multiple scattering of waves in the time-domain:
A tutorial
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Wave scattering; Multiple scattering; Frequency-domain; Time-domain;
Particles
ID HIGH-FREQUENCY SCATTERING; ELECTROMAGNETIC SCATTERING;
RADIATIVE-TRANSFER; DIRECTIONAL RADIOMETRY; TRANSPARENT SPHERE;
CONFIGURATIONS; TRANSMISSION; REFLECTION; SYSTEMS; LIGHT
AB The equations for frequency-domain multiple scattering are derived for a scalar or electromagnetic plane wave incident on a collection of particles at known positions, and in the time-domain for a plane wave pulse incident on the same collection of particles. The calculation is carried out for five different combinations of wave types and particle types of increasing geometrical complexity. The results are used to illustrate and discuss a number of physical and mathematical characteristics of multiple scattering in the frequency- and time-domains. We argue that frequency-domain multiple scattering is a purely mathematical construct since there is no temporal sequencing information in the frequency-domain equations and since the multi-particle path information can be dispelled by writing the equations in another mathematical form. However, multiple scattering becomes a definite physical phenomenon in the time-domain when the collection of particles is illuminated by an appropriately short localized pulse. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Lock, James A.] Cleveland State Univ, Dept Phys, Cleveland, OH 44115 USA.
[Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Lock, JA (reprint author), Cleveland State Univ, Dept Phys, Cleveland, OH 44115 USA.
EM j.lock@csuohio.edu
FU NASA
FX We thank two anonymous reviewers for their constructive and helpful
comments. MIM appreciates support from the NASA Remote Sensing Theory
Program managed by Lucia Tsaoussi and the NASA Radiation Sciences
Program managed by Hal Maring.
NR 55
TC 3
Z9 3
U1 1
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 SEP
PY 2015
VL 162
SI SI
BP 221
EP 240
DI 10.1016/j.jqsrt.2015.02.023
PG 20
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA CM2WU
UT WOS:000357543800024
ER
PT J
AU Wu, AS
Xiong, XX
Jin, ZH
Lukashin, C
Wenny, BN
Butler, JJ
AF Wu, Aisheng
Xiong, Xiaoxiong
Jin, Zhonghai
Lukashin, Constantine
Wenny, Brian N.
Butler, James J.
TI Sensitivity of Intercalibration Uncertainty of the CLARREO Reflected
Solar Spectrometer Features
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Climate Absolute Radiance and Refractivity Observatory (CLARREO);
intercalibration; MODerate resolution Imaging Spectroradiometer (MODIS);
radiometry; spectral reflectance; Visible Infrared Imaging Radiometer
Suite (VIIRS)
ID SCIAMACHY; CLOUD
AB The Climate Absolute Radiance and Refractivity Observatory (CLARREO) mission was recommended by the National Research Council in 2007 to conduct highly accurate and International System of Unit-traceable decadal change observations and provide an on-orbit intercalibration standard with high accuracy for relevant Earth observing sensors. The goal of reference intercalibration is to enable rigorous observations of critical climate change variables, including reflected broadband radiation, cloud properties, and changes in surface albedo, including snow and ice albedo feedback, to be made consistently among different sensors. This requires the CLARREO Reflected Solar Spectrometer (RSS) to provide highly accurate spectral reflectance measurements to establish an on-orbit reference with a radiometric accuracy requirement better than 0.3% (k = 2) for existing sensors. In this paper, MODTRAN-simulated top-of-atmosphere spectral data and spectral measurements from the SCIAMACHY instrument on Envisat are used to determine sensitivity of intercalibration uncertainty on key design parameters of the CLARREO spectrometer: spectral range, sampling and resolution. Their impact on intercalibration uncertainty for MODIS and VIIRS imagers is estimated for various surface types (ocean, vegetation, desert, snow, deep convective clouds, clouds and all-sky). Results indicate that for the visible to near-infrared spectral region (465-856 nm), the RSS instrument under current design concept produces uncertainties of 0.16% for the spectral range and 0.3% for the sampling and resolution. However, for the water vapor absorption bands in the short wavelength infrared region (1242-1629 nm), the same requirement is not met for sampling and resolution due to their high sensitivity to the influence of atmospheric water vapor.
C1 [Wu, Aisheng; Wenny, Brian N.] Sigma Space Corp, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong; Butler, James J.] NASA, Sci & Explorat Directorate, GSFC, Greenbelt, MD 20771 USA.
[Jin, Zhonghai] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Jin, Zhonghai; Lukashin, Constantine] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
RP Wu, AS (reprint author), Sigma Space Corp, Lanham, MD 20706 USA.
EM aisheng.wu@ssaihq.com
RI Richards, Amber/K-8203-2015
FU NASA CLARREO project
FX This work was supported by the NASA CLARREO project.
NR 14
TC 1
Z9 1
U1 2
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2015
VL 53
IS 9
BP 4741
EP 4751
DI 10.1109/TGRS.2015.2409030
PG 11
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA CK4AJ
UT WOS:000356159000002
ER
PT J
AU Lavalle, M
Hensley, S
AF Lavalle, Marco
Hensley, Scott
TI Extraction of Structural and Dynamic Properties of Forests From
Polarimetric-Interferometric SAR Data Affected by Temporal Decorrelation
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Decorrelation; interferometry; polarimetry; synthetic aperture radar
(SAR)
ID SYNTHETIC-APERTURE RADAR; POL-INSAR DATA; L-BAND; HEIGHT ESTIMATION;
UNDERLYING TOPOGRAPHY; SCATTERING MECHANISMS; PARAMETER-ESTIMATION; 1ST
DEMONSTRATION; BOREAL FOREST; POLINSAR DATA
AB This paper addresses the important yet unresolved problem of estimating forest properties from polarimetric-interferometric radar images affected by temporal decorrelation. We approach the problem by formulating a physical model of the polarimetric-interferometric coherence that incorporates both volumetric and temporal decorrelation effects. The model is termed random-motion-over-ground (RMoG) model, as it combines the random-volume-over-ground (RVoG) model with a Gaussian-statistic motion model of the canopy elements. Key features of the RMoG model are: 1) temporal decorrelation depends on the vertical structure of forests; 2) volumetric and temporal coherences are not separable as simple multiplicative factors; and 3) temporal decorrelation is complex-valued and changes with wave polarization. This third feature is particularly important as it allows compensating for unknown levels of temporal decorrelation using multiple polarimetric channels. To estimate model parameters such as tree height and canopy motion, we propose an algorithm that minimizes the least square distance between model predictions and complex coherence observations. The algorithm was applied to L-band NASA's Uninhabited Aerial Vehicle Synthetic Aperture Radar data acquired over the Harvard Forest (Massachussetts, USA). We found that the RMS difference at stand level between estimated RMoG-model tree height and NASA's lidar Laser Vegetation and Ice Sensor tree height was within 12% of the lidar-derived height, which improved significantly the RMS difference of 37% obtained using the RVoG model and ignoring temporal decorrelation. This result contributes to our ability of estimating forest biomass using in-orbit and forthcoming polarimetric-interferometric radar missions.
C1 [Lavalle, Marco; Hensley, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lavalle, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM marco.lavalle@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology, under
National Aeronautics and Space Administration
FX This work was supported by the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration.
NR 77
TC 4
Z9 4
U1 3
U2 16
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2015
VL 53
IS 9
BP 4752
EP 4767
DI 10.1109/TGRS.2015.2409066
PG 16
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA CK4AJ
UT WOS:000356159000003
ER
PT J
AU Daniels, JL
Smith, GL
Priestley, KJ
Thomas, S
AF Daniels, Janet L.
Smith, G. Louis
Priestley, Kory J.
Thomas, Susan
TI Using Lunar Observations to Validate In-Flight Calibrations of Clouds
and the Earth's Radiant Energy System Instruments
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aqua; calibration; Clouds and the Earth's Radiant Energy System (CERES);
Earth Observing System; Earth radiation budget; lunar measurements;
Moon; radiometry; remote sensing; satellites; telescope; Terra;
validation
AB The validation of in-orbit instrument performance requires both stability in calibration source and also calibration corrections to compensate for instrument changes. Unlike internal calibrations, the Moon offers an external source whose signal variance is predictable and nondegrading. This paper describes a method of validation using lunar observations scanning near full moon by the Clouds and the Earth's Radiant Energy System (CERES) Flight Model (FM)-1 and FM-2 aboard the Terra satellite, FM-3 and FM-4 aboard the Aqua satellite, and, as of 2012, FM-5 aboard Suomi National Polar-orbiting Partnership. Given the stability of the source, adjustments within the data set are based entirely on removing orbital effects. Lunar observations were found to require a consistent data set spanning at least two to three years in length to examine instrument stability due to the final step when lunar libration effects are addressed. Initial results show a 20% annual variability in the data set. Using this method, however, results show trends per data channel of 1.0% per decade or less for FM-1 through FM-4. Results for FM-5 are not included in this paper because a sufficient data record has not yet been collected.
C1 [Daniels, Janet L.] NASA, Langley Res Ctr, Hampton, VA 23666 USA.
[Smith, G. Louis; Thomas, Susan] Sci Syst & Applicat Inc, NASA, Langley Res Ctr, Hampton, VA 23666 USA.
[Priestley, Kory J.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23666 USA.
RP Daniels, JL (reprint author), NASA, Langley Res Ctr, Hampton, VA 23666 USA.
EM janet.l.daniels@nasa.gov; george.l.smith@nasa.gov;
kory.j.priestley@nasa.gov; susan.thomas-1@nasa.gov
FU Science Directorate of Langley Research Center; Science Mission
Directorate of the Earth Science Division of NASA
FX The authors would like to thank Science Directorate of Langley Research
Center and the Science Mission Directorate of the Earth Science Division
of NASA for the support of the CERES Project.
NR 11
TC 4
Z9 4
U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD SEP
PY 2015
VL 53
IS 9
BP 5110
EP 5116
DI 10.1109/TGRS.2015.2417314
PG 7
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA CK4AJ
UT WOS:000356159000030
ER
PT J
AU Kwon, Y
Toure, AM
Yang, ZL
Rodell, M
Picard, G
AF Kwon, Yonghwan
Toure, Ally M.
Yang, Zong-Liang
Rodell, Matthew
Picard, Ghislain
TI Error Characterization of Coupled Land Surface-Radiative Transfer Models
for Snow Microwave Radiance Assimilation
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Error characteristics; land-surfacemodel (LSM); microwave brightness
temperature; radiative transfer model (RTM); snow
ID EMISSION MODEL; BRIGHTNESS TEMPERATURE; LAYERED SNOWPACKS; SEASONAL
SNOW; COVER; SYSTEM; STRATIGRAPHY; SIMULATIONS; SCATTERING; EVOLUTION
AB Snow microwave radiance assimilation (RA) or brightness temperature data assimilation (DA) has shown promise for improving snow water equivalent (SWE) estimation. A successful RA study requires, however, an analysis of the error characteristics of coupled land surface-radiative transfer models (LSM/RTMs). This paper focuses on the Community Land Model version 4 (CLM4) as the land-surface model and on the microwave emission model for layered snowpacks (MEMLS) and the dense media radiative transfer multilayer (DMRT-ML) model as RTMs. Using the National Aeronautics and Space Administration Cold Land Processes Field Experiment (CLPX) data sets and through synthetic experiments, the errors of the coupled CLM4/DMRT-ML and CLM4/MEMLS are characterized by: 1) evaluating the CLM4 snowpack state simulations; 2) assessing the performance of RTMs in simulating the brightness temperature (T-B); and 3) analyzing the correlations between the SWE error (epsilon_SWE) and the T-B error (epsilon_T-B) from the RA perspective. The results using the CLPX data sets show that, given a large error of the snow grain radius (epsilon_re) under dry snowpack conditions (along with a small error of the snow temperature (epsilon_T-snow)), the correlations between epsilon_SWE and epsilon_T-B are mainly determined by the relationship between epsilon_r(e) and the snow depth error (epsilon_d(snow)) or the snow density error (epsilon_rho(snow)). The synthetic experiments were carried out for the CLPX region (shallow snowpack conditions) and the Rocky Mountains (deep snowpack conditions) using the atmospheric ensemble reanalysis produced by the coupled DA Research Testbed/Community Atmospheric Model (CAM4). The synthetic experiments support the results from the CLPX data sets and show that the errors of soil (the water content and the temperature), snow wetness, and snow temperature mostly result in positive correlations between epsilon_SWE and epsilon_T-B. CLM4/DMRT-ML and CLM4/MEMLS tend to produce varying RA performance, with more positive and negative correlations between epsilon_SWE and epsilon_T-B, respectively. These results suggest the necessity of using multiple snowpack RTMs in RA to improve the SWE estimation at the continental scale. The results in this paper also show that the magnitude of epsilon_r(e) and its relationship to epsilon_SWE are important for the RA performance. Most of the SWE estimations in RA are improved when epsilon_SWE and epsilon_r(e) show a high positive correlation (greater than 0.5).
C1 [Kwon, Yonghwan; Yang, Zong-Liang] Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, Austin, TX 78712 USA.
[Toure, Ally M.; Rodell, Matthew] NASA Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Toure, Ally M.] Univ Space Res Assoc, NASA Goddard Earth Sci Technol & Res GESTAR, Columbia, MD 21046 USA.
[Yang, Zong-Liang] Univ Texas Austin, Jackson Sch Geosci, Ctr Integrated Earth Syst Sci, Austin, TX 78712 USA.
[Picard, Ghislain] Univ Grenoble 1, Lab Glaciol & Geophys Environm, F-38041 Grenoble, France.
RP Yang, ZL (reprint author), Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, Austin, TX 78712 USA.
EM yhkwon@utexas.edu; ally.mouniroutoure@nasa.gov; liang@jsg.utexas.edu;
matthew.rodell@nasa.gov; ghislain.picard@ujf-grenoble.fr
RI Rodell, Matthew/E-4946-2012; Yang, Zong-Liang/B-4916-2011; Picard,
Ghislain/D-4246-2013
OI Rodell, Matthew/0000-0003-0106-7437; Picard,
Ghislain/0000-0003-1475-5853
FU Jackson School of Geosciences, The University of Texas at Austin (UT
Austin)
FX The authors would like to thank the Jackson School of Geosciences, The
University of Texas at Austin (UT Austin) for providing the travel funds
to visit the National Aeronautics and Space Administration Goddard Space
Flight Center, C. Matzler and M. Durand for providing their computer
codes, and all of the Cold Land Processes Field Experiment (CLPX)
participants for collecting the data used in this paper. The authors
would also like to thank M. Durand and M. Flanner for their discussions
on the Community Land Model version 4 (CLM4) snow grain radius
simulations and P. A. Bobeck for language assistance. The Data
Assimilation Research Testbed (DART)/Community Atmospheric Model (CAM4)
atmospheric ensemble reanalysis data are prepared by K. Raeder
(raeder@ucar.edu). The computational resources were provided by the UT
Texas Advanced Computing Center.
NR 55
TC 4
Z9 4
U1 2
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 SEP
PY 2015
VL 53
IS 9
BP 5247
EP 5268
DI 10.1109/TGRS.2015.2419977
PG 22
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA CK4AJ
UT WOS:000356159000042
ER
PT J
AU Henderson, B
Werner, M
AF Henderson, Brenda
Werner, Mark
TI An experimental investigation of overexpanded jets with chevrons
SO JOURNAL OF SOUND AND VIBRATION
LA English
DT Article
ID SHOCK-ASSOCIATED NOISE; CONVERGENT-DIVERGENT NOZZLES; SUPERSONIC JETS;
AXISYMMETRICAL JET; TABS; FIELD; FLOW
AB Results are presented for experiments investigating the impact of chevrons on over-expanded and subsonic jet plumes and associated acoustic radiation. Faceted, bi-conic convergent-divergent nozzles with design Mach numbers equal to 1.51 and 1.65 are used in the experiments. A design space of nine chevrons with a range of penetrations, lengths and widths are investigated. Low-penetration chevrons are shown to have limited impact on broadband and shock-associated noise for all jet Mach numbers investigated. High-penetration chevrons produce significant peak-noise reduction (relative to the baseline nozzle) in the peak-jet-noise direction with greater noise reduction for subsonic than for supersonic exhausts. High-penetration chevrons are found to increase broadband-shock-associated noise for the highest Mach number jet investigated. While particle image velocimetry results indicate chevrons introduce axial vorticity at all jet conditions, the associated mixing is limited for supersonic exhausts relative to that for subsonic exhausts due to the strong and periodic radial velocity components associated with the jet-shock-cell structure. The introduction of chevrons modifies the near-nozzle shock-cell structure and the impact of internally (within the nozzle) generated shocks on the shock-cell structure generated in the jet plume. The modifications in the near-nozzle shock-cell structure can lead to increased broadband-shock-associated-noise levels for some operating conditions. Published by Elsevier Ltd.
C1 [Henderson, Brenda; Werner, Mark] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Henderson, B (reprint author), NASA, Glenn Res Ctr, MS 54-3,21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM brenda.s.henderson@nasa.gov; mark.p.wernet@nasa.gov
FU Strategic Environmental Research and Development Program; NASA's
Supersonics Project in the Fundamental Aeronautics Program
FX The authors acknowledge the diligent and resourceful efforts of Dr.
Randy Locke and Dr. Adam Wroblewski in the acquisition of the
cross-stream Ply data, The authors also thank the staff of AeroAcoustic
Propulsion Laboratory at NASA Glenn Research Center. The work was funded
by the Strategic Environmental Research and Development Program and by
NASA's Supersonics Project in the Fundamental Aeronautics Program.
NR 42
TC 1
Z9 1
U1 2
U2 11
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0022-460X
EI 1095-8568
J9 J SOUND VIB
JI J. Sound Vibr.
PD SEP 1
PY 2015
VL 351
BP 119
EP 142
DI 10.1016/j.jsv.2015.04.020
PG 24
WC Acoustics; Engineering, Mechanical; Mechanics
SC Acoustics; Engineering; Mechanics
GA CJ5UX
UT WOS:000355558300009
ER
PT J
AU Wiesner, VL
Bansal, NP
AF Wiesner, Valerie L.
Bansal, Narottarn P.
TI Mechanical and thermal properties of calcium-magnesium aluminosilicate
(CMAS) glass
SO JOURNAL OF THE EUROPEAN CERAMIC SOCIETY
LA English
DT Article
DE CMAS; Glass; Dilatometry; Viscosity; Mechanical properties
ID ENVIRONMENTAL BARRIER COATINGS; CERAMIC-MATRIX COMPOSITES; DEPOSITS;
DELAMINATION; DEGRADATION; TEMPERATURE; SUBJECT; ENGINES; SYSTEMS; MODEL
AB Thermal stability of a synthetic sand composition, which was developed as a simulant for calcium magnesium aluminosilicate (CMAS) turbine deposits, was characterized using thermogravimetric and differential thermal analysis (TG/DTA). The sand was melted into CMAS glass, which had a composition of 23.3CaO-6.4MgO-3.1Al(2)O(3)-62.5SiO(2)-4.1Na(2)O-0.5K(2)O-0.04Fe(2)O(3) (mol.%), determined by inductively coupled plasma atomic emission spectroscopy (ICP-AES). Bulk density of the glass was measured to be 2.63 g/cm(3), and the Young's and shear moduli were 84.3 GPa and 33.6 GPa, respectively, along with a Poisson's ratio of 0.26. Vickers microhardness and indentation fracture toughness were determined to be 6.14 +/- 0.1 GPa and 0.70 +/- 0.05 MPa m(1/2), respectively. Glass transition temperature, softening point and coefficient of thermal expansion of the glass were measured by dilatometry. Glass viscosities were estimated over a temperature range of 600-1500 degrees C using dilatometric reference points of the glass and from composition-based methods. Times required for infiltration of molten CMAS glass into thermal or environmental bather coatings were also estimated. Published by Elsevier Ltd.
C1 [Wiesner, Valerie L.; Bansal, Narottarn P.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
RP Wiesner, VL (reprint author), NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
EM valerie.l.wiesner@nasa.gov
FU NASA's Transformative Tools and Technologies (TTT) Project of the
Transformative Aeronautics Concept Program (TCAP) as well as through
NASA's Pathways Program
FX The authors are grateful to Dr. Bryan Harder, Dr. Dongming Zhu, Dr. Nate
Jacobson and Dr. Jim Smialek for helpful discussions, Mr. Dereck Johnson
for thermal analysis, Dr. Paul Angel for melting the synthetic sand into
glass and Mr. Ralph Pawlik for mechanical testing. This research was
supported by NASA's Transformative Tools and Technologies (TTT) Project
of the Transformative Aeronautics Concept Program (TCAP) as well as
through NASA's Pathways Program.
NR 35
TC 5
Z9 5
U1 7
U2 66
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0955-2219
EI 1873-619X
J9 J EUR CERAM SOC
JI J. Eur. Ceram. Soc.
PD SEP
PY 2015
VL 35
IS 10
BP 2907
EP 2914
DI 10.1016/j.jeurceramsoc.2015.03.032
PG 8
WC Materials Science, Ceramics
SC Materials Science
GA CJ2ZS
UT WOS:000355353800020
ER
PT J
AU Cerracchio, P
Gherlone, M
Di Sciuva, M
Tessler, A
AF Cerracchio, Priscilla
Gherlone, Marco
Di Sciuva, Marco
Tessler, Alexander
TI A novel approach for displacement and stress monitoring of sandwich
structures based on the inverse Finite Element Method
SO COMPOSITE STRUCTURES
LA English
DT Article
DE Sandwich structures; Shape sensing; Stress sensing; Inverse Finite
Element Method
ID SHEAR-DEFORMATION-THEORY; GRATING STRAIN SENSORS; LAMINATED COMPOSITE;
PLATE ELEMENT; SHAPE; SHELLS; RECONSTRUCTION; VIBRATION
AB The real-time reconstruction of the displacement and stress fields from discrete-location strain measurements is a fundamental feature for monitoring systems, which is generally referred to as shape- and stress-sensing. Presented herein is a computationally efficient shape- and stress-sensing methodology that is ideally suited for applications to laminated composite and sandwich structures. The new approach employs the inverse Finite Element Method (iFEM) as a general framework and the Refined Zigzag Theory (RZT) as the underlying plate theory. Using a C-0-discretization, a three-node inverse plate finite element is formulated. The element formulation enables robust and efficient modeling of plate structures instrumented with strain sensors that have arbitrary positions. The methodology leads to a set of linear algebraic equations that are solved efficiently for the unknown nodal displacements. These displacements are then used at the finite element level to compute full-field strains and stresses that may be in turn used to assess structural integrity. Numerical results for multilayered, highly heterogeneous laminates demonstrate the unique capability of this new formulation for shape- and stress-sensing. (C) 2015 Elsevier Ltd. All rights reserved.
C1 [Cerracchio, Priscilla; Gherlone, Marco; Di Sciuva, Marco] Politecn Torino, Dept Mech & Aerosp Engn, I-10129 Turin, Italy.
[Tessler, Alexander] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
RP Cerracchio, P (reprint author), Politecn Torino, Dept Mech & Aerosp Engn, Corso Duca Abruzzi 24, I-10129 Turin, Italy.
EM priscilla.cerracchio@polito.it; marco.gherlone@polito.it;
marco.disciuva@polito.it; Alexander.Tessler-1@nasa.gov
OI Gherlone, Marco/0000-0002-5711-0046
FU National Institute of Aerospace (NIA); NASA Langley research Center,
Hampton, Virginia
FX The authors Priscilla Cerracchio, Marco Gherlone and Marco Di Sciuva
would like to thank for their support the National Institute of
Aerospace (NIA) and NASA Langley research Center, Hampton, Virginia.
NR 48
TC 5
Z9 6
U1 1
U2 20
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 SEP 1
PY 2015
VL 127
BP 69
EP 76
DI 10.1016/j.compstruct.2015.02.081
PG 8
WC Materials Science, Composites
SC Materials Science
GA CH6IH
UT WOS:000354139800008
ER
PT J
AU Yoder, DA
DeBonis, JR
Georgiadis, NJ
AF Yoder, D. A.
DeBonis, J. R.
Georgiadis, N. J.
TI Modeling of turbulent free shear flows
SO COMPUTERS & FLUIDS
LA English
DT Review
DE Jet flow; Mixing layers; Turbulence models; Compressibility effects;
Temperature effects; Propulsion
ID COMPRESSIBLE MIXING LAYER; LARGE-EDDY SIMULATION; PLANAR
VELOCITY-MEASUREMENTS; PRESSURE-STRAIN CORRELATION; FINITE-DIFFERENCE
SCHEMES; REYNOLDS-NUMBER; BOUNDARY-LAYER; GROWTH-RATE; PARALLEL STREAMS;
MACH NUMBER
AB The modeling of turbulent free shear flows is crucial to the simulation of many aerospace applieations, yet often receives less attention than the modeling of wall boundary layers. Thus, while turbulence model development in general has proceeded very slowly in the past twenty years, progress for free shear flows has been even more so. This paper highlights some of the fundamental issues in modeling free shear flows for propulsion applications, presents a review of past modeling efforts, and identifies areas where further research is needed. Among the topics discussed are differences between planar and axisymmetric flows, development versus self-similar regions, the effect of compressibility and the evolution of compressibility corrections, the effect of temperature on jets, and the significance of turbulent Prandtl and Schmidt numbers for reacting shear flows. Large-eddy simulation greatly reduces the amount of empiricism in the physical modeling, but is sensitive to a number of numerical issues. This paper includes an overview of the importance of numerical scheme, mesh resolution, boundary treatment, sub-grid modeling, and filtering in conducting a successful simulation. Published by Elsevier Ltd.
C1 [Yoder, D. A.; DeBonis, J. R.; Georgiadis, N. J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP DeBonis, JR (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM dennis.a.yoder@nasa.gov; james.r.debonis@nasa.gov;
nicholas.j.georgiadis@nasa.gov
NR 144
TC 3
Z9 3
U1 2
U2 19
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0045-7930
EI 1879-0747
J9 COMPUT FLUIDS
JI Comput. Fluids
PD AUG 31
PY 2015
VL 117
BP 212
EP 232
DI 10.1016/j.compfluid.2015.05.009
PG 21
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA CN2RL
UT WOS:000358269500018
ER
PT J
AU Love, JJ
Rigler, EJ
Pulkkinen, A
Riley, P
AF Love, Jeffrey J.
Rigler, E. Joshua
Pulkkinen, Antti
Riley, Pete
TI On the lognormality of historical magnetic storm intensity statistics:
Implications for extreme-event probabilities
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SELF-ORGANIZED CRITICALITY; SPACE WEATHER; SOLAR-WIND; POWER LAWS; D-ST;
DISTRIBUTIONS; DST; FIELD
AB An examination is made of the hypothesis that the statistics of magnetic storm maximum intensities are the realization of a lognormal stochastic process. Weighted least squares and maximum likelihood methods are used to fit lognormal functions to -Dst storm time maxima for years 1957-2012; bootstrap analysis is used to established confidence limits on forecasts. Both methods provide fits that are reasonably consistent with the data; both methods also provide fits that are superior to those that can be made with a power-law function. In general, the maximum likelihood method provides forecasts having tighter confidence intervals than those provided by weighted least squares. From extrapolation of maximum likelihood fits: a magnetic storm with intensity exceeding that of the 1859 Carrington event, -Dst >= 850 nT, occurs about 1.13 times per century and a wide 95% confidence interval of [0.42, 2.41] times per century; a 100 year magnetic storm is identified as having a -Dst >= 880 nT (greater than Carrington) but a wide 95% confidence interval of [490, 1187] nT.
C1 [Love, Jeffrey J.; Rigler, E. Joshua] US Geol Survey, Geomagnetism Program, Denver, CO 80225 USA.
[Pulkkinen, Antti] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Riley, Pete] Predict Sci Inc, San Diego, CA USA.
RP Love, JJ (reprint author), US Geol Survey, Geomagnetism Program, Box 25046, Denver, CO 80225 USA.
EM jlove@usgs.gov
OI Riley, Pete/0000-0002-1859-456X
FU USGS Geomagnetism Program
FX We thank C.A. Finn, J. McCarthy, M.P. Moschetti, and J.L. Slate for
reviewing a draft manuscript. We thank M.A. Balikhin and A. Kelbert for
useful conversations. This work was supported by the USGS Geomagnetism
Program. The standard Dst index is provided by the Kyoto World Data
Center in Japan (wdc.kugi.kyoto-u.ac.jp).
NR 63
TC 7
Z9 7
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2015
VL 42
IS 16
BP 6544
EP 6553
DI 10.1002/2015GL064842
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA CU3FY
UT WOS:000363410800002
ER
PT J
AU Bramson, AM
Byrne, S
Putzig, NE
Sutton, S
Plaut, JJ
Brothers, TC
Holt, JW
AF Bramson, Ali M.
Byrne, Shane
Putzig, Nathaniel E.
Sutton, Sarah
Plaut, Jeffrey J.
Brothers, T. Charles
Holt, John W.
TI Widespread excess ice in Arcadia Planitia, Mars
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MEDUSAE FOSSAE FORMATION; IMPACT CRATERS; GROUND ICE; SUBSURFACE ICE;
EQUATORIAL ICE; STABILITY; DEPOSITS; SURFACE; DRY; SUBLIMATION
AB The distribution of subsurface water ice on Mars is a key constraint on past climate, while the volumetric concentration of buried ice (pore-filling versus excess) provides information about the process that led to its deposition. We investigate the subsurface of Arcadia Planitia by measuring the depth of terraces in simple impact craters and mapping a widespread subsurface reflection in radar sounding data. Assuming that the contrast in material strengths responsible for the terracing is the same dielectric interface that causes the radar reflection, we can combine these data to estimate the dielectric constant of the overlying material. We compare these results to a three-component dielectric mixing model to constrain composition. Our results indicate a widespread, decameters-thick layer that is excess water ice similar to 10(4) km(3) in volume. The accumulation and long-term preservation of this ice is a challenge for current Martian climate models.
C1 [Bramson, Ali M.; Byrne, Shane; Sutton, Sarah] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Putzig, Nathaniel E.] SW Res Inst, Boulder, CO USA.
[Plaut, Jeffrey J.] Jet Prop Lab, Pasadena, CA USA.
[Brothers, T. Charles; Holt, John W.] Univ Texas Austin, Inst Geophys, Austin, TX USA.
RP Bramson, AM (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM bramson@lpl.arizona.edu
OI Brothers, Thomas/0000-0002-8043-7987
FU NSF [DGE-1143953]
FX SHARAD radar tracks were processed using the Colorado SHARAD Processing
System (CO-SHARPS) and analyzed using geophysical interpretation
software provided courtesy of SeisWare International Inc. Access to the
CO-SHARPS processing boutique can be requested at
https://www.boulder.swri.edu/sharad.php. All HiRISE and CTX images used
are publically available through NASA's Planetary Data System
(https://pds.nasa.gov/). Eight of the digital terrain models A.M.B.
created for this project have been archived and released to the public
(http://www.uahirise.org/dtm/), and the other three DTMs will be
released by January 2016. We benefitted from insightful conversations
from Hanna Sizemore, David Stillman, and James T. Keane. A.M.B. was
supported by the NSF Graduate Research Fellowship under grant
DGE-1143953.
NR 52
TC 6
Z9 6
U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2015
VL 42
IS 16
BP 6566
EP 6574
DI 10.1002/2015GL064844
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CU3FY
UT WOS:000363410800005
ER
PT J
AU Le Mevel, H
Feigl, KL
Cordova, L
DeMets, C
Lundgren, P
AF Le Mevel, Helene
Feigl, Kurt L.
Cordova, Loreto
DeMets, Charles
Lundgren, Paul
TI Evolution of unrest at Laguna del Maule volcanic field (Chile) from
InSAR and GPS measurements, 2003 to 2014
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SURFACE DEFORMATION; CAMPI FLEGREI; RADAR INTERFEROGRAMS; CENTRAL ANDES;
HALF-SPACE; CALDERA; EARTHQUAKE; CALIFORNIA; UPLIFT; CONSTRAINTS
AB The Laguna del Maule (LdM) volcanic field in the southern volcanic zone of the Chilean Andes exhibits a large volume of rhyolitic material erupted during postglacial times (20-2 ka). Since 2007, LdM has experienced an unrest episode characterized by high rates of deformation. Analysis of new GPS and Interferometric Synthetic Aperture Radar (InSAR) data reveals uplift rates greater than 190 mm/yr between January 2013 and November 2014. The geodetic data are modeled as an inflating sill at depth. The results are used to calculate the temporal evolution of the vertical displacement. The best time function for modeling the InSAR data set is a double exponential model with rates increasing from 2007 through 2010 and decreasing slowly since 2010. We hypothesize that magma intruding into an existing silicic magma reservoir is driving the surface deformation. Modeling historical uplift at Yellowstone, Long Valley, and Three Sisters volcanic fields suggests a common temporal evolution of vertical displacement rates.
C1 [Le Mevel, Helene; Feigl, Kurt L.; DeMets, Charles] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Cordova, Loreto] SERNAGEOMIN, Observ Volcanol Los Andes Sur, Temuco, Chile.
[Lundgren, Paul] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Le Mevel, H (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
EM lemevel@wisc.edu
RI Feigl, Kurt/E-8106-2012
OI Feigl, Kurt/0000-0002-2059-6708
FU NASA [NNX12AO37G]; U.S. National Science Foundation [EAR-1411779]; Weeks
family; G.P. Woollard fund
FX We thank the RAMSAC CORS Network from Instituto Geografico Nacional de
Argentina for access to their GPS data, which were used for part of this
study. We thank Christophe Vigny and Jaime Campos of the International
Associated Laboratory Montessus de Ballore (LIA-MB) for sharing GPS data
from station MAUL. We appreciate the logistical assistance generously
provided by Carlos Cardona and Fernando Gil at OVDAS, as well as
Francisco Delgado, and Tor Stetson-Lee. We are especially grateful to
"Don Luis" Torres for his gracious hospitality and nautical expertise.
We also thank Nathan Andersen, Brad Singer, Elena Baluyut, Tabrez Ali,
and the "LdM team" for helpful discussions. Detailed reviews from
Michael Poland, Matthew Pritchard, and Francisco Delgado improved the
manuscript. This research was partially supported by grants from NASA
(NNX12AO37G), U.S. National Science Foundation (EAR-1411779), as well as
support from the Weeks family and the G.P. Woollard fund. We acknowledge
SAR data from the following space agencies: ASI (COSMO-Skymed), DLR
(TSX), JAXA (ALOS), ESA (ERS and ENVISAT), and NASA (UAVSAR), as well as
the coordination by the Supersites Initiative. The Generic Mapping Tool
software was used to produce several maps [Wessel and Smith, 1998]. The
authors thank Michael Poland, Francisco Delgado, and Matthew Pritchard
for their assistance in critically and constructively evaluating this
paper.
NR 40
TC 5
Z9 5
U1 3
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2015
VL 42
IS 16
BP 6590
EP 6598
DI 10.1002/2015GL064665
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CU3FY
UT WOS:000363410800008
ER
PT J
AU Wu, XP
Heflin, MB
AF Wu, Xiaoping
Heflin, Michael B.
TI A global assessment of accelerations in surface mass transport
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID DEFORMATION; VARIABILITY; BALANCE; EARTH
AB Water mass transport in the Earth's dynamic surface layer of atmosphere, cryosphere, and hydrosphere driven by various global change processes has complex spatiotemporal patterns. Here we determine global patterns and regional mean values of accelerations in surface mass variations during the Gravity Recovery and Climate Experiment (GRACE) mission's data span from 2002.2 to 2015.0. GRACE gravity data are supplemented by surface deformation from 607 Global Navigation Satellite System stations, an ocean bottom pressure model, satellite laser ranging, and loose a priori knowledge on mass variation regimes incorporating high-resolution geographic boundaries. While Greenland and West Antarctica have strong negative accelerations, Alaska and the Arctic Ocean show significant positive accelerations. In addition, the accelerations are not constant in time with some regions showing considerable variability due to irregular interannual changes. No evidence of significant nonsteric mean sea level acceleration has been found, but the uncertainty is quite large.
C1 [Wu, Xiaoping; Heflin, Michael B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Wu, XP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Xiaoping.Wu@jpl.nasa.gov
FU NASA
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration (NASA), and funded through NASA's GRACE Science
Team and Interdisciplinary Research in Earth Science programs. We thank
John Ries for providing calibrated GRACE data covariance matrices and
for discussion; Shin-Chan Han for providing the coseismic gravity change
patterns; and Srinivas Bettadpur, Jeffrey Freymueller, and Chris Larsen
for discussions. SLR C20 time series are from Minkang Cheng. GRACE level
2 data are publicly available from http://podaac.jpl.nasa.gov/grace/.
GNSS and JPL ECCO time series are publicly available from
http://sideshow.jpl.nasa.gov/post/series.html and
http://ecco.jpl.nasa.gov, respectively. Degree 1 time series generated
are available from the authors upon request. The Generic Mapping Tools
(GMT) are used to create Figure 2. Two anonymous reviewers provided
valuable comments and suggestions.
NR 19
TC 1
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U1 1
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 AUG 28
PY 2015
VL 42
IS 16
BP 6716
EP 6723
DI 10.1002/2015GL064941
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CU3FY
UT WOS:000363410800024
ER
PT J
AU Williams, AP
Seager, R
Abatzoglou, JT
Cook, BI
Smerdon, JE
Cook, ER
AF Williams, A. Park
Seager, Richard
Abatzoglou, John T.
Cook, Benjamin I.
Smerdon, Jason E.
Cook, Edward R.
TI Contribution of anthropogenic warming to California drought during
2012-2014
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID DATA ASSIMILATION SYSTEM; UNITED-STATES; CLIMATE-CHANGE; ATMOSPHERIC
CONTROLS; GLOBAL DROUGHT; SEVERITY INDEX; TEMPERATURE; WATER;
VARIABILITY; GROUNDWATER
AB A suite of climate data sets and multiple representations of atmospheric moisture demand are used to calculate many estimates of the self-calibrated Palmer Drought Severity Index, a proxy for near-surface soil moisture, across California from 1901 to 2014 at high spatial resolution. Based on the ensemble of calculations, California drought conditions were record breaking in 2014, but probably not record breaking in 2012-2014, contrary to prior findings. Regionally, the 2012-2014 drought was record breaking in the agriculturally important southern Central Valley and highly populated coastal areas. Contributions of individual climate variables to recent drought are also examined, including the temperature component associated with anthropogenic warming. Precipitation is the primary driver of drought variability but anthropogenic warming is estimated to have accounted for 8-27% of the observed drought anomaly in 2012-2014 and 5-18% in 2014. Although natural variability dominates, anthropogenic warming has substantially increased the overall likelihood of extreme California droughts.
C1 [Williams, A. Park; Seager, Richard; Cook, Benjamin I.; Smerdon, Jason E.; Cook, Edward R.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Abatzoglou, John T.] Univ Idaho, Dept Geog, Moscow, ID 83843 USA.
[Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Williams, AP (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
EM williams@ldeo.columbia.edu
RI Smerdon, Jason/F-9952-2011; Williams, Park/B-8214-2016; Cook,
Benjamin/H-2265-2012;
OI Williams, Park/0000-0001-8176-8166; Abatzoglou, John/0000-0001-7599-9750
FU NSF [AGS-1243204]; NOAA [NA14OAR4310232]
FX We thank Y. Mao for sharing VIC meteorological forcing and soil moisture
data from Mao et al. [2015]. We thank J. Sheffield for making the SHEFF
data set available at http://hydrology.princeton.edu. We thank R. Vose
for providing the VOSE data set. PRISM data were obtained from the PRISM
Climate Group, Oregon State University
(http://www.prism.oregonstate.edu, created 4 February 2004). PRISM dew
point data were obtained from http://oldprism.nacse.org. TopoWx data
were obtained from ftp://mco.cfc.umt.edu/resources/TopoWx-source/. LDAS
data were obtained from http://disc.sci.gsfc.nasa.gov/hydrology/data
holdings. GPCC data through 2013 come from
ftp://ftp.dwd.de/pub/data/gpcc/html/fulldata_v7_doi_download.html.
PREC/L, NCEP2, NCEP/NCAR, NOAA twentieth century reanalysis, and GPCC
for 2014 were accessed from http://www.esrl.noaa.gov. A spatially
continuous map of soil moisture holding capacities for the United States
came from the Web Soil Survey data set
(http://websoilsurvey.nrcs.usda.gov). This work was supported by NSF
award AGS-1243204 and NOAA award NA14OAR4310232. Lamont-Doherty
publication number 7924. Thanks to K.J. Anchukaitis and two anonymous
reviewers for comments that improved this manuscript. The climate and
PDSIsc data sets compiled for this study are available at
http://www.ldeo.columbia.edu/similar to
williams/ca_drought_2015_grl.html.
NR 71
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2015
VL 42
IS 16
BP 6819
EP 6828
DI 10.1002/2015GL064924
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA CU3FY
UT WOS:000363410800037
ER
PT J
AU Coats, S
Smerdon, JE
Seager, R
Griffin, D
Cook, BI
AF Coats, Sloan
Smerdon, Jason E.
Seager, Richard
Griffin, Daniel
Cook, Benjamin I.
TI Winter-to-summer precipitation phasing in southwestern North America: A
multicentury perspective from paleoclimatic model-data comparisons
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LAST MILLENNIUM; TREE-RING; UNITED-STATES; VARIABILITY; MONSOON;
SURFACE; DROUGHT; CLIMATE; RECONSTRUCTIONS; SIMULATIONS
AB The phasing of winter-to-summer precipitation anomalies in the North American monsoon (NAM) region 2 (113.25 degrees W-107.75 degrees W, 30 degrees N-35.25 degrees N-NAM2) of southwestern North America is analyzed in fully coupled simulations of the Last Millennium and compared to tree ring reconstructed winter and summer precipitation variability. The models simulate periods with in-phase seasonal precipitation anomalies, but the strength of this relationship is variable on multidecadal time scales, behavior that is also exhibited by the reconstructions. The models, however, are unable to simulate periods with consistently out-of-phase winter-to-summer precipitation anomalies as observed in the latter part of the instrumental interval. The periods with predominantly in-phase winter-to-summer precipitation anomalies in the models are significant against randomness, and while this result is suggestive of a potential for dual-season drought on interannual and longer time scales, models do not consistently exhibit the persistent dual-season drought seen in the dendroclimatic reconstructions. These collective findings indicate that model-derived drought risk assessments may underestimate the potential for dual-season drought in 21st century projections of hydroclimate in the American Southwest and parts of Mexico.
C1 [Coats, Sloan; Smerdon, Jason E.; Seager, Richard; Cook, Benjamin I.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Coats, Sloan] Columbia Univ, Dept Earth & Environm Sci, New York, NY USA.
[Griffin, Daniel] Univ Minnesota, Dept Geog Environm & Soc, Minneapolis, MN USA.
[Griffin, Daniel] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Coats, S (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
EM sjc2164@columbia.edu
RI Smerdon, Jason/F-9952-2011; Cook, Benjamin/H-2265-2012
FU NOAA [NA11OAR4310166]; NSF [AGS-1243204]; National Aeronautics and Space
Administration Modeling Analysis and Prediction Program [WBS
281945.02.04.02.74]; NOAA Climate and Global Change Postdoctoral
Fellowship
FX This work was supported by NOAA award NA11OAR4310166 and NSF award
AGS-1243204. Additional support for B.I. Cook was provided by National
Aeronautics and Space Administration Modeling Analysis and Prediction
Program WBS 281945.02.04.02.74 ("Cool and Warm Season Moisture
Reconstruction and Modeling over North America"). Additional support for
D. Griffin was provided by the NOAA Climate and Global Change
Postdoctoral Fellowship. We acknowledge the World Climate Research
Programme's Working Group on Coupled Modelling, which is responsible for
CMIP, and we thank the climate modeling groups (listed in Table 1) for
producing and making available their model output. For CMIP the U.S.
Department of Energy's Program for Climate Model Diagnosis and
Intercomparison provides coordinating support and led development of
software infrastructure in partnership with the Global Organization for
Earth System Science Portal. The data for this paper are available from
the Program for Climate Model Diagnosis and Intercomparison
(http://cmip-pcmdi.llnl.gov/cmip5/). LDEO contribution 7917. We thank
three anonymous reviewers for their comments that improved the quality
of this manuscript. We, further, thank Haibo Liu and Naomi Henderson for
their considerable computational support.
NR 42
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U1 4
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2015
VL 120
IS 16
BP 8052
EP 8064
DI 10.1002/2015JD023085
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU3KX
UT WOS:000363425200003
ER
PT J
AU Savtchenko, AK
Huffman, G
Vollmer, B
AF Savtchenko, Andrey K.
Huffman, George
Vollmer, Bruce
TI Assessment of precipitation anomalies in California using TRMM and MERRA
data
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID EL-NINO; WATER; PATTERNS; ENERGY
AB Using modern satellite (Tropical Rainfall Measuring Mission, TRMM, 1998-2014) and reanalysis (Modern-Era Retrospective Analysis for Research and Applications, MERRA, 1979-2015) data, we reassess certain aspects of the precipitation climate in California from the past decades. California has a well-pronounced rain season that peaks in December-February. However, the 95% confidence interval around the climatological precipitation during these months imply that deviations on the order of 60% of the expected amounts are very likely during the most important period of the rain season. While these positive and negative anomalies alternate almost every year and tend to cancel each other, severe multiyear declines of precipitation in California appear on decadal scales. The 1986-1994 decline of precipitation was similar to the current one that started in 2011 and is apparent in the reanalysis data. In terms of accumulated deficits of precipitation, that episode was no less severe than the current one. While El Nino (the warm phase of the El Nino-Southern Oscillation, ENSO) is frequently cited as the natural forcing expected to bring a relief from drought, our assessment is that ENSO has been driving at best only 6% of precipitation variability in California in the past three decades. Using fractional risk analysis of precipitation during typical versus drying periods, we show that the likelihood of losing the most intensive precipitation events drastically increases during the multiyear drying events. Storms delivering up to 50% of the precipitation in California are driven by atmospheric rivers making landfall. However, these phenomena can be suppressed and even blocked by persistent ridges of atmospheric pressure in the northeast Pacific. The reanalysis and satellite data are proven to be reliable to the extent where they yield information on developing conditions and observed precipitation anomalies.
C1 [Savtchenko, Andrey K.] NASA, Goddard Space Flight Ctr, ADNET Syst, Greenbelt, MD 20771 USA.
[Huffman, George; Vollmer, Bruce] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Savtchenko, AK (reprint author), NASA, Goddard Space Flight Ctr, ADNET Syst, Code 610-2, Greenbelt, MD 20771 USA.
EM Candrey.savtchenko@nasa.gov
RI Huffman, George/F-4494-2014
OI Huffman, George/0000-0003-3858-8308
NR 28
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U1 3
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2015
VL 120
IS 16
BP 8206
EP 8215
DI 10.1002/2015JD023573
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU3KX
UT WOS:000363425200012
ER
PT J
AU Lee, J
Hsu, NC
Bettenhausen, C
Sayer, AM
Seftor, CJ
Jeong, MJ
AF Lee, Jaehwa
Hsu, N. Christina
Bettenhausen, Corey
Sayer, Andrew M.
Seftor, Colin J.
Jeong, Myeong-Jae
TI Retrieving the height of smoke and dust aerosols by synergistic use of
VIIRS, OMPS, and CALIOP observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SKY RADIANCE MEASUREMENTS; OPTICAL-PROPERTIES; VERTICAL PROFILE; GLOBAL
OCEAN; AERONET; MODIS; ALGORITHM; DEPTH; MODELS; MISR
AB This study extends the application of the previously developed Aerosol Single-scattering albedo and layer Height Estimation (ASHE) algorithm, which was originally applied to smoke aerosols only, to both smoke and dust aerosols by including nonspherical dust properties in the retrieval process. The main purpose of the algorithm is to derive aerosol height information over wide areas using aerosol products from multiple satellite sensors simultaneously: aerosol optical depth (AOD) and Angstrom exponent from the Visible Infrared Imaging Radiometer Suite (VIIRS), UV aerosol index from the Ozone Mapping and Profiler Suite (OMPS), and total backscatter coefficient profile from the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP). The case studies suggest that the ASHE algorithm performs well for both smoke and dust aerosols, showing root-mean-square error of the retrieved aerosol height as compared to CALIOP observations from 0.58 to 1.31 km and mean bias from -0.70 to 1.13 km. In addition, the algorithm shows the ability to retrieve single-scattering albedo to within 0.03 of Aerosol Robotic Network inversion data for moderate to thick aerosol loadings (AOD of similar to 1.0). For typical single-layered aerosol cases, the estimated uncertainty in the retrieved height ranges from 1.20 to 1.80 km over land and from 1.15 to 1.58 km over ocean when favorable conditions are met. Larger errors are observed for multilayered aerosol events, due to the limited sensitivities of the passive sensors to such cases.
C1 [Lee, Jaehwa; Hsu, N. Christina; Bettenhausen, Corey; Sayer, Andrew M.; Seftor, Colin J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lee, Jaehwa] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Bettenhausen, Corey; Seftor, Colin J.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Sayer, Andrew M.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Jeong, Myeong-Jae] Gangneung Wonju Natl Univ, Dept Atmospher & Environm Sci, Kangnung, Gangwon, South Korea.
RP Lee, J (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM jaehwa.lee@nasa.gov
RI Sayer, Andrew/H-2314-2012;
OI Sayer, Andrew/0000-0001-9149-1789; Lee, Jaehwa/0000-0002-5029-476X
FU NASA's EOS program
FX This project is funded by the NASA's EOS program, managed by H. Maring.
The VIIRS, OMPS, and CALIOP science teams are gratefully acknowledged
for their efforts to create and maintain the data records used in this
investigation. We thank the PIs and managers (I. Abboud, M. Anderson, J.
C. Antuqa Marrero, W. P. Arnott, V. E. Cachorro Revilla, C. Coburn, A.
L. Contreras, A. Cooper, J. Csavina, P. Disterhoft, V. Fioletov, G. A.
Fouts, R. Frouin, H. Fuelberg, G. Gimmestad, B. Gingrey, E. Gonzalez, W.
M. Hao, J. Herman, R. M. Hoff, B. N. Holben, P. Ionov, M. Ivey, F.
Javier, S. Jones, T. Kampe, K. Knupp, G. Labow, B. Lefer, C. Lehmann, G.
Lesins, D. Moore, A. H. Omar, N. O'Neill, T. H. Painter, S. Piazzolla,
B. Pierce, A. Predoi-Cross, K. Repasky, A. Royer, G. P. Robertson, J. A.
Shaw, J. Sherman, G. Stensaas, J. Stutz, D. Tanre, M. Tzortziou, J. van
den Bosch, R. Wagener, C. Walthall, and J. Zhang) for establishing and
maintaining the AERONET sites. Ping Yang at Texas A&M University is also
acknowledged for providing the single-scattering property database for
tri-axial ellipsoidal particles. The VIIRS data were obtained from the
NASA Atmosphere Science Investigator-led Processing Systems (SIPS)
(sips.ssec.wisc.edu/flo/search/), the OMPS data from the website of the
NASA OMPS science team (https://ozoneaq.gsfc.nasa.gov/data/omps/), the
CALIOP data from the NASA Langley Research Center Atmospheric Science
Data Center (https://eosweb.larc.nasa.gov/order-data/), and the AERONET
data from the AERONET website (http://aeronet.gsfc.nasa.gov).
NR 53
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Z9 3
U1 3
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2015
VL 120
IS 16
BP 8372
EP 8388
DI 10.1002/2015JD023567
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU3KX
UT WOS:000363425200023
ER
PT J
AU Yang, Q
Easter, RC
Campuzano-Jost, P
Jimenez, JL
Fast, JD
Ghan, SJ
Wang, HL
Berg, LK
Barth, MC
Liu, Y
Shrivastava, MB
Singh, B
Morrison, H
Fan, JW
Ziegler, CL
Bela, M
Apel, E
Diskin, GS
Mikoviny, T
Wisthaler, A
AF Yang, Qing
Easter, Richard C.
Campuzano-Jost, Pedro
Jimenez, Jose L.
Fast, Jerome D.
Ghan, Steven J.
Wang, Hailong
Berg, Larry K.
Barth, Mary C.
Liu, Ying
Shrivastava, Manishkumar B.
Singh, Balwinder
Morrison, Hugh
Fan, Jiwen
Ziegler, Conrad L.
Bela, Megan
Apel, Eric
Diskin, Glenn S.
Mikoviny, Tomas
Wisthaler, Armin
TI Aerosol transport and wet scavenging in deep convective clouds: A case
study and model evaluation using a multiple passive tracer analysis
approach
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SIMULATED SQUALL LINE; WRF-CHEM; MARINE STRATOCUMULUS; SPECTRUM
FORMATION; MASS-SPECTROMETER; SOUTHEAST PACIFIC; REGIONAL AEROSOL;
CUMULUS CLOUDS; CLIMATE MODEL; VOCALS-REX
AB Wet scavenging of aerosols by continental deep convective clouds is studied for a supercell storm complex observed over Oklahoma during the Deep Convective Clouds and Chemistry campaign. A new passive-tracer-based transport analysis framework is developed to characterize convective transport using vertical profiles of several passive trace gases. For this case, the analysis estimates that observed passive gas mixing ratios in the upper troposphere convective outflow consist of 47% low level (<3km) inflow air, 32% entrained midtroposphere air, and 21% upper troposphere air. The new analysis framework is used to estimate aerosol wet scavenging efficiencies. Observations yield high overall scavenging efficiencies of 81% for submicron aerosol mass. Organic, sulfate, and ammonium aerosols have similar wet scavenging efficiencies (80%-84%). The apparent scavenging efficiency for nitrate aerosol is much lower (57%), but the scavenging efficiency for nitrate aerosol plus nitric acid combined (84%) is close to the other species. Scavenging efficiencies for aerosol number are high for larger particles (84% for 0.15-2.5 mu m diameter) but are lower for smaller particles (64% for 0.03-0.15 mu m). The storm is simulated using the chemistry version of the Weather Research and Forecasting model. Compared to the observation-based analysis, the standard model strongly underestimates aerosol scavenging efficiencies by 32% and 41% in absolute differences for submicron mass and number. Adding a new treatment of secondary activation significantly improves simulated aerosol scavenging, producing wet scavenging efficiencies that are only 7% and 8% lower than observed efficiencies. This finding emphasizes the importance of secondary activation for aerosol wet removal in deep convective storms.
C1 [Yang, Qing; Easter, Richard C.; Fast, Jerome D.; Ghan, Steven J.; Wang, Hailong; Berg, Larry K.; Liu, Ying; Shrivastava, Manishkumar B.; Singh, Balwinder; Fan, Jiwen] Pacific NW Natl Lab, Richland, WA 99352 USA.
[Campuzano-Jost, Pedro; Jimenez, Jose L.; Bela, Megan] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
[Campuzano-Jost, Pedro; Jimenez, Jose L.; Bela, Megan] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Barth, Mary C.; Morrison, Hugh; Apel, Eric] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Ziegler, Conrad L.] Natl Severe Storms Lab, Norman, OK 73069 USA.
[Diskin, Glenn S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Mikoviny, Tomas] Oak Ridge Associated Univ, Oak Ridge, TN USA.
[Wisthaler, Armin] Univ Innsbruck, Inst Ion Phys & Appl Phys, A-6020 Innsbruck, Austria.
RP Yang, Q (reprint author), Pacific NW Natl Lab, Richland, WA 99352 USA.
EM qing.yang@pnnl.gov
RI Wang, Hailong/B-8061-2010; Jimenez, Jose/A-5294-2008; Berg,
Larry/A-7468-2016; Yang, Qing/H-3275-2011; Ghan, Steven/H-4301-2011;
Fan, Jiwen/E-9138-2011
OI Wang, Hailong/0000-0002-1994-4402; Jimenez, Jose/0000-0001-6203-1847;
Berg, Larry/0000-0002-3362-9492; Yang, Qing/0000-0003-2067-5999; Ghan,
Steven/0000-0001-8355-8699;
FU Office of Science of the U.S. Department of Energy as part of the
Atmospheric System Research Program; NASA [NNX12AC03G]; NSF
[AGS-1360834, AGS-1063945]; Austrian Federal Ministry for Transport,
Innovation and Technology (bmvit) through the Austrian Space
Applications Programme of the Austrian Research Promotion Agency (FFG);
NASA Postdoctoral Program (NPP); National Science Foundation; National
Science Foundation (NSF); National Aeronautics and Space Administration
(NASA); Deutsches Zentrum fur Luft- und Raumfahrt; National Oceanic and
Atmospheric Administration; [DE-AC06-76RLO 1830]
FX The DC3 data set is available to download from the NASA LARC site:
https://www-air.larc.nasa.gov/cgi-bin/ArcView/dc3-seac4rs#3. The
modeling data are available by contacting the corresponding author at
qing.yang@pnnl.gov. This research was supported by the Office of Science
of the U.S. Department of Energy as part of the Atmospheric System
Research Program. The Pacific Northwest National Laboratory is operated
by Battelle Memorial Institute under contract DE-AC06-76RLO 1830. We
thank Elaine Chapman for providing helpful editorial comments. We would
like to express our gratitude toward Anderson Bruce, Lee Thornhill, and
Gao Chen from NASA Langley; Allen Schanot and Jorgen Jensen from UCAR;
Sara Lance and Paul Lawson from SPEC, Inc., and Milos Markovic from
CIRES for providing the valuable measurement data and/or for their
guidance on the processing of the data. We thank Zhe Feng at PNNL and
Xiquan Dong at the University of North Dakota for providing access to
the data set. P.C.J. and J.L.J. were supported by NASA NNX12AC03G and
NSF AGS-1360834. Acetone and benzene measurements on the DC8 were
supported by the Austrian Federal Ministry for Transport, Innovation and
Technology (bmvit) through the Austrian Space Applications Programme of
the Austrian Research Promotion Agency (FFG). T.M. acknowledges funding
through the NASA Postdoctoral Program (NPP). The Mosaic NEXRAD radar
data set is produced by the National Severe Storms Laboratory (NSSL)
National Mosaic and QPE Project (now Multi-Radar Multi-Sensor, or
http://nmq.ou.edu). The NSSL mobile environmental soundings were
obtained during DC3 with support from NSF grant AGS-1063945. The
National Center for Atmospheric Research is sponsored by the National
Science Foundation. The National Science Foundation (NSF), the National
Aeronautics and Space Administration (NASA), the Deutsches Zentrum fur
Luft- und Raumfahrt, and the National Oceanic and Atmospheric
Administration are gratefully acknowledged for sponsoring the DC3 field
experiment.
NR 63
TC 9
Z9 9
U1 0
U2 18
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2015
VL 120
IS 16
BP 8448
EP 8468
DI 10.1002/2015JD023647
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU3KX
UT WOS:000363425200027
ER
PT J
AU Liaskos, CE
Allen, DJ
Pickering, KE
AF Liaskos, Christina E.
Allen, Dale J.
Pickering, Kenneth E.
TI Sensitivity of tropical tropospheric composition to lightning NOx
production as determined by replay simulations with GEOS-5
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OPTICAL TRANSIENT DETECTOR; OZONE MONITORING INSTRUMENT;
NITROGEN-OXIDES; ATMOSPHERIC CHEMISTRY; VERTICAL-DISTRIBUTION; GLOBAL
DISTRIBUTION; TRANSPORT MODELS; GENERATED NOX; CMAQ MODEL; STERAO-A
AB The sensitivity of tropical tropospheric composition to the source strength of nitrogen oxides (NOx) produced by lightning (LNOx) is analyzed for September through November 2007 using the NASA GEOS-5 model constrained by MERRA fields, with full GMI stratospheric-tropospheric chemistry and an LNOx algorithm that is appropriate for use in a climate modeling setting; satellite retrievals from OMI, TES, and OMI/MLS; and in situ measurements from SHADOZ ozonesondes. Global mean LNOx production rates of 0 to 492 mol NO flash(-1) and the subsequent responses of NOx, ozone (O-3), hydroxyl radical (OH), nitric acid (HNO3), peroxyacetyl nitrate (PAN), and NOy (NOx + HNO3 + PAN) are investigated. The radiative implications associated with LNOx-induced changes in tropospheric O-3 are assessed. Increasing the LNOx production rate by a factor of 4 (from 123 to 492 mol flash(-1)) leads to tropical upper tropospheric enhancements of greater than 100% in NOx, OH, HNO3, and PAN. This increase in LNOx production also leads to O-3 enhancements of up to 60%, which subsequently yields a factor-of-three increase in the mean net radiative flux at the tropopause. An LNOx source of 246 mol flash(-1) agrees reasonably well with measurements, with an approximate factor-of-two uncertainty due to the short length of the study, inconsistencies in the observational data sets, and systematic biases in modeled LNOx production. Further research into the regional dependencies of lightning flash rates and LNOx production per flash, along with improvements in satellite retrievals, should help resolve the discrepancies that currently exist between the model and observations.
C1 [Liaskos, Christina E.; Allen, Dale J.; Pickering, Kenneth E.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Liaskos, CE (reprint author), NIST, Gaithersburg, MD 20899 USA.
EM christina.liaskos@nist.gov
RI Pickering, Kenneth/E-6274-2012; Allen, Dale/F-7168-2010
OI Allen, Dale/0000-0003-3305-9669
FU NASA Modeling and Analysis Program [NASA/NNX09AJ37G]; NASA's Modeling,
Analysis and Prediction (MAP) program
FX The data used for the results of this paper are available from the
author upon request. This work was supported by NASA Modeling and
Analysis Program grant NASA/NNX09AJ37G. The GEOS-5 model system is
developed and maintained in the Global Modeling and Assimilation Office
at NASA GSFC under funding from NASA's Modeling, Analysis and Prediction
(MAP) program. The CCM is a joint development, led by the Atmospheric
Chemistry and Dynamics Laboratory and the GMAO. Simulations are
performed on the High-Performance Computing environment at the NASA
Center for Climate Simulation (NCCS) at NASA GSFC. We appreciate the
contributions of many GMAO staff toward the development of GEOS-5. In
particular, Eric Nielsen was instrumental in both the development of the
coupled chemistry capability and in the implementation of the lightning
parameterization that is the subject of this manuscript. Andrea Molod
directed the GEOS-5 GCM simulations that provided training data for the
flash rate parameterization and helped interpret the output. Lawrence
Takacs, Max Suarez, Arlindo DaSilva, and Atanas Tryanov were all
instrumental in the development of the GEOS-5 replay capability. The
feedback based on the analysis of the transport of tracers, performed by
Lesley Ott, aided in the understanding of model errors which led to
improvements in tracer transport. We also gratefully acknowledge the
contributions to the GEOS-5 infrastructure of Atanas Tryanov, Matt
Thompson, and Ben Auer, which made the AGCM tractable and portable to
different platforms. We thank X. Liu for providing the OMI level-2 ozone
profile data sets, and we thank J. Ziemke for the OMI/MLS tropospheric
column ozone data product.
NR 87
TC 5
Z9 5
U1 1
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 27
PY 2015
VL 120
IS 16
BP 8512
EP 8534
DI 10.1002/2014JD022987
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CU3KX
UT WOS:000363425200030
ER
PT J
AU Barge, LM
Cardoso, SSS
Cartwright, JHE
Cooper, GJT
Cronin, L
De Wit, A
Doloboff, IJ
Escribano, B
Goldstein, RE
Haudin, F
Jones, DEH
Mackay, AL
Maselko, J
Pagano, JJ
Pantaleone, J
Russell, MJ
Sainz-Diaz, CI
Steinbock, O
Stone, DA
Tanimoto, Y
Thomas, NL
AF Barge, Laura M.
Cardoso, Silvana S. S.
Cartwright, Julyan H. E.
Cooper, Geoffrey J. T.
Cronin, Leroy
De Wit, Anne
Doloboff, Ivria J.
Escribano, Bruno
Goldstein, Raymond E.
Haudin, Florence
Jones, David E. H.
Mackay, Alan L.
Maselko, Jerzy
Pagano, Jason J.
Pantaleone, J.
Russell, Michael J.
Ignacio Sainz-Diaz, C.
Steinbock, Oliver
Stone, David A.
Tanimoto, Yoshifumi
Thomas, Noreen L.
TI From Chemical Gardens to Chemobrionics
SO CHEMICAL REVIEWS
LA English
DT Review
ID CITY HYDROTHERMAL FIELD; INORGANIC PRECIPITATE MEMBRANES; SCALE TUBULAR
ARCHITECTURES; REACTION-DIFFUSION SYSTEMS; PORTLAND-CEMENT HYDRATION;
CATION-EXCHANGE MEMBRANE; BRONSTED ACID CATALYST; OF-LIFE EXPERIMENTS;
SILICA TUBES; SEMIPERMEABLE-MEMBRANE
C1 [Barge, Laura M.; Doloboff, Ivria J.; Russell, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cardoso, Silvana S. S.] Univ Cambridge, Dept Chem Engn & Biotechnol, Cambridge CB2 3RA, England.
[Cartwright, Julyan H. E.; Ignacio Sainz-Diaz, C.] Univ Granada, Inst Andaluz Ciencias Tierra, CSIC, E-18100 Granada, Spain.
[Cooper, Geoffrey J. T.; Cronin, Leroy] Univ Glasgow, WestCHEM Sch Chem, Glasgow G12 8QQ, Lanark, Scotland.
[De Wit, Anne; Haudin, Florence] Univ Libre Bruxelles, Nonlinear Phys Chem Unit, B-1050 Brussels, Belgium.
[Escribano, Bruno] Basque Ctr Appl Math, E-48009 Bilbao, Spain.
[Goldstein, Raymond E.] Univ Cambridge, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England.
[Jones, David E. H.] Univ Newcastle Tyne, Dept Chem, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England.
[Mackay, Alan L.] Univ London, Birkbeck Coll, London WC1E 7HX, England.
[Maselko, Jerzy] Univ Alaska Anchorage, Dept Chem, Anchorage, AK 99508 USA.
[Pagano, Jason J.] Saginaw Valley State Univ, Dept Chem, Univ Ctr, Saginaw, MI 48710 USA.
[Pantaleone, J.] Univ Alaska Anchorage, Dept Phys, Anchorage, AK 99508 USA.
[Steinbock, Oliver] Florida State Univ, Dept Chem & Biochem, Tallahassee, FL 32306 USA.
[Stone, David A.] Iron Shell LLC, Tucson, AZ 85717 USA.
[Tanimoto, Yoshifumi] Osaka Ohtani Univ, Fac Pharm, Tondabayashi 5488540, Japan.
[Thomas, Noreen L.] Univ Loughborough, Dept Mat, Loughborough LE11 3TU, Leics, England.
RP Cartwright, JHE (reprint author), Univ Granada, Inst Andaluz Ciencias Tierra, CSIC, E-18100 Granada, Spain.
EM julyan.cartwright@csic.es; steinbck@chem.fsu.edu
RI Goldstein, Raymond/F-2932-2011; Cartwright, Julyan/C-1387-2016;
OI Goldstein, Raymond/0000-0003-2645-0598; Cartwright,
Julyan/0000-0001-7392-0957; Cronin, Lee/0000-0001-8035-5757
FU U.S. National Science Foundation [CHE-0608631, DMR-1005861]; Spanish
Ministerio de Ciencia e Innovacion [FIS2013-48444-C2-2-P]; Andalusian
PAIDI group [RNM363]; NASA Astrobiology Institute (Icy Worlds)
FX We thank Shawn McGlynn, Paul Davies, and Fabian Brau for useful
discussions. We acknowledge the U.S. National Science Foundation, Grants
CHE-0608631 and DMR-1005861, the Spanish Ministerio de Ciencia e
Innovacion Grant FIS2013-48444-C2-2-P, and the Andalusian PAIDI group
Grant RNM363. L.M.B., and MJ.R's research 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 the NASA Astrobiology Institute (Icy Worlds). We acknowledge
useful discussions within the NAI-sponsored Thermodynamics
Disequilibrium and Evolution Focus Group. This review has emerged from
the discussions held at the Lorentz Center workshop on Chemical Gardens,
7-11 May 2012, Leiden organized by Julyan Cartwright, Michael Russell,
and Oliver Steinbock; we thank the Lorentz Center staff for their
wonderful support.
NR 275
TC 34
Z9 34
U1 9
U2 70
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0009-2665
EI 1520-6890
J9 CHEM REV
JI Chem. Rev.
PD AUG 26
PY 2015
VL 115
IS 16
BP 8652
EP 8703
DI 10.1021/acs.chemrev.5b00014
PG 52
WC Chemistry, Multidisciplinary
SC Chemistry
GA CQ0XH
UT WOS:000360321300011
PM 26176351
ER
PT J
AU Soebiyanto, RP
Gross, D
Jorgensen, P
Buda, S
Bromberg, M
Kaufman, Z
Prosenc, K
Socan, M
Alonso, TV
Widdowson, MA
Kiang, RK
AF Soebiyanto, Radina P.
Gross, Diane
Jorgensen, Pernille
Buda, Silke
Bromberg, Michal
Kaufman, Zalman
Prosenc, Katarina
Socan, Maja
Alonso, Tomas Vega
Widdowson, Marc-Alain
Kiang, Richard K.
TI Associations between Meteorological Parameters and Influenza Activity in
Berlin (Germany), Ljubljana (Slovenia), Castile and Leon (Spain) and
Israeli Districts
SO PLOS ONE
LA English
DT Article
AB Background
Studies in the literature have indicated that the timing of seasonal influenza epidemic varies across latitude, suggesting the involvement of meteorological and environmental conditions in the transmission of influenza. In this study, we investigated the link between meteorological parameters and influenza activity in 9 sub-national areas with temperate and subtropical climates: Berlin (Germany), Ljubljana (Slovenia), Castile and Leon (Spain) and all 6 districts in Israel.
Methods
We estimated weekly influenza-associated influenza-like-illness (ILI) or Acute Respiratory Infection (ARI) incidence to represent influenza activity using data from each country's sentinel surveillance during 2000-2011 (Spain) and 2006-2011 (all others). Meteorological data was obtained from ground stations, satellite and assimilated data. Two generalized additive models (GAM) were developed, with one using specific humidity as a covariate and another using minimum temperature. Precipitation and solar radiation were included as additional covariates in both models. The models were adjusted for previous weeks' influenza activity, and were trained separately for each study location.
Results
Influenza activity was inversely associated (p<0.05) with specific humidity in all locations. Minimum temperature was inversely associated with influenza in all 3 temperate locations, but not in all subtropical locations. Inverse associations between influenza and solar radiation were found in most locations. Associations with precipitation were location-dependent and inconclusive. We used the models to estimate influenza activity a week ahead for the 2010/2011 period which was not used in training the models. With exception of Ljubljana and Israel's Haifa District, the models could closely follow the observed data especially during the start and the end of epidemic period. In these locations, correlation coefficients between the observed and estimated ranged between 0.55 to 0.91and the model-estimated influenza peaks were within 3 weeks from the observations.
Conclusion
Our study demonstrated the significant link between specific humidity and influenza activity across temperate and subtropical climates, and that inclusion of meteorological parameters in the surveillance system may further our understanding of influenza transmission patterns.
C1 [Soebiyanto, Radina P.] Univ Space Res Associat, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Soebiyanto, Radina P.; Kiang, Richard K.] NASA Goddard Space Flight Ctr, Global Change Data Ctr, Greenbelt, MD 20771 USA.
[Gross, Diane; Jorgensen, Pernille] WHO, Reg Off Europe, DK-2100 Copenhagen, Denmark.
[Gross, Diane; Widdowson, Marc-Alain] US Ctr Dis Control & Prevent CDC, Influenza Div, Atlanta, GA USA.
[Buda, Silke] Robert Koch Inst, Berlin, Germany.
[Bromberg, Michal; Kaufman, Zalman] Minist Hlth, Israel Ctr Dis Control, Tel Hashomer, Israel.
[Prosenc, Katarina] Natl Inst Publ Hlth Slovenia, Virol Lab, Ljubljana, Slovenia.
[Socan, Maja] Natl Inst Publ Hlth, Communicable Dis & Environm Hlth Care, Ljubljana, Slovenia.
[Alonso, Tomas Vega] Publ Hlth Directorate, Dept Hlth, Valladolid, Spain.
RP Kiang, RK (reprint author), NASA Goddard Space Flight Ctr, Global Change Data Ctr, Greenbelt, MD 20771 USA.
EM richard.k.kiang@nasa.gov
FU NASA Applied Sciences Public Health program; CDC Influenza Division
FX This study was supported by NASA Applied Sciences Public Health program
and CDC Influenza Division. The funders had no role in study design,
data collection and analysis, decision to publish, or preparation of the
manuscript.
NR 0
TC 0
Z9 0
U1 0
U2 4
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 AUG 26
PY 2015
VL 10
IS 8
AR e0134701
DI 10.1371/journal.pone.0134701
PG 21
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CP7LO
UT WOS:000360069400031
PM 26309214
ER
PT J
AU Smialek, JL
AF Smialek, James L.
TI Compiled furnace cyclic lives of EB-PVD thermal barrier coatings
SO SURFACE & COATINGS TECHNOLOGY
LA English
DT Article
DE Thermal barrier coatings; Cyclic oxidation; Superalloys; Spallation;
Aluminides
ID SINGLE-CRYSTAL SUPERALLOYS; TBC SYSTEMS; BOND COATS; SCALE ADHESION;
AL2O3 SCALE; FAILURE; MECHANISMS; LIFETIME; PLATINUM; SPALLATION
AB Furnace cycling has been widely used to study the failure of EB-PVD thermal barrier coatings. This contribution compiles TBC furnace cyclic lives over a broad literature base to highlight optimum systems and generalized trends not always apparent in one study. Systems included typical bond coats (Pt-modified aluminides, diffused Pt-only gamma/gamma', and NiCoCrAlY (+/- Pt, Hf) overlays) and superalloy substrates (1st, 2nd, 3rd generation single crystals, directionally solidified, or conventionally cast). Pretreatments included controlled low p(O-2) bond coat pre-oxidation and grit blasting (or none). The aggregate lives (similar to 70) suggest a general trend with temperature, similar to 10-fold decrease for every 100 degrees C increase. Measured alumina scale thicknesses (similar to 30) were, on average, similar to 6.1 +/- 1.8 mu m at failure and independent of temperature for conventional systems. Most failures thus occurred in less time than that predicted to grow 7 mu m of alumina scale (as estimated from separate TGA studies of a Pt-modified aluminide coated 2nd generation single crystal superalloy). A tentative activation energy indicated from the broad distribution of failure times was similar to 280 kJ/mol, while that from homogeneous TGA testing was similar to 380 kJ/mol, with regression coefficients of r(2) = 0.57 and 0.98, respectively. Published by Elsevier B.V.
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Smialek, JL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM James.L.Smialek@nasa.gov
FU NASA
FX The author is grateful for helpful comments and shared information from
Drs. U. Schulz, G. Meier, D. Zhu, and B. Pint. Ken Murphy (Alcoa/Howmet)
is acknowledged for producing the Pt-modified aluminide coatings for TGA
testing. This work was supported by the NASA Fundamental Aeronautics
Program.
NR 54
TC 5
Z9 5
U1 6
U2 18
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0257-8972
J9 SURF COAT TECH
JI Surf. Coat. Technol.
PD AUG 25
PY 2015
VL 276
BP 31
EP 38
DI 10.1016/j.surfcoat.2015.06.018
PG 8
WC Materials Science, Coatings & Films; Physics, Applied
SC Materials Science; Physics
GA CQ4SJ
UT WOS:000360594600005
ER
PT J
AU Grebenkemper, JH
Hu, YF
Barrett, D
Gogna, P
Huang, CK
Bux, SK
Kauzlarich, SM
AF Grebenkemper, Jason H.
Hu, Yufei
Barrett, Dashiel
Gogna, Pawan
Huang, Chen-Kuo
Bux, Sabah K.
Kauzlarich, Susan M.
TI High Temperature Thermoelectric Properties of Yb14MnSb11 Prepared from
Reaction of MnSb with the Elements
SO CHEMISTRY OF MATERIALS
LA English
DT Article
ID INTERNATIONAL ROUND-ROBIN; SPACE POWER APPLICATIONS;
TRANSPORT-PROPERTIES; INTERMETALLIC COMPOUNDS; BULK THERMOELECTRICS;
SEEBECK COEFFICIENT; ZINTL COMPOUNDS; PERFORMANCE; SUBLIMATION; GROWTH
AB Compounds of the Yb14MnSb11 structure type are the highest efficiency bulk p-type materials for high temperature thermoelectric applications, with reported figures of merit (ZTs) as high as similar to 1.3 at 1275 K. Further optimization of ZT for this structure type is possible with the development of a simple synthetic route. However, this has been difficult to achieve because of the small amount of Mn required compared with Yb and Sb. A simple synthetic route for Yb14MnSb11 has been developed utilizing a combination of ball milling and annealing to produce phase-pure material followed by spark plasma sintering for consolidation. The materials have been characterized by powder X-ray diffraction before and after spark plasma sintering. The stoichiometric reaction of Yb, Sb, and MnSb provides phase-pure powder by X-ray diffraction. Upon cycling to temperatures greater than 1272 K, Yb14MnSb11 shows the presence of Yb11Sb10. Additional samples with 5% and 10% excess Mn were also investigated. Adding 5-10% excess Mn does not change the low temperature properties and improves the high temperature ZT, resulting in a ZT of 1.1-1.2 at 1000 K for Yb14Mn1.05Sb11, 30-40% improvement over that of the Sn flux reaction. The increase in ZT is attributed to optimization of the carrier concentration. These results provide a reliable method of bulk synthesis of this Zintl phase and open the way for discovery of new compounds with potential for even higher ZT.
C1 [Grebenkemper, Jason H.; Hu, Yufei; Barrett, Dashiel; Kauzlarich, Susan M.] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA.
[Gogna, Pawan; Huang, Chen-Kuo; Bux, Sabah K.] CALTECH, Jet Prop Lab, Thermal Energy Convers Technol Grp, Pasadena, CA 91109 USA.
RP Kauzlarich, SM (reprint author), Univ Calif Davis, Dept Chem, One Shields Ave, Davis, CA 95616 USA.
EM smkauzlarich@ucdavis.edu
FU U.S. Department of Energy, Office of Science, Office of Basic Energy
Sciences [DE-AC02-06CH11357]; NEUP; National Aeronautics and Space
Administration; NASA Science Mission Directorate's Radioisotope Power
Systems
FX Use of the Advanced Photon Source at Argonne National Laboratory was
supported by the U.S. Department of Energy, Office of Science, Office of
Basic Energy Sciences, under Contract No. DE-AC02-06CH11357. Financial
support from NEUP is gratefully acknowledged. 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. This work was supported by the NASA Science Mission
Directorate's Radioisotope Power Systems. We thank Thierry Caillat for
the ATEC sample and data.
NR 38
TC 8
Z9 9
U1 8
U2 54
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0897-4756
EI 1520-5002
J9 CHEM MATER
JI Chem. Mat.
PD AUG 25
PY 2015
VL 27
IS 16
BP 5791
EP 5798
DI 10.1021/acs.chemmater.5b02446
PG 8
WC Chemistry, Physical; Materials Science, Multidisciplinary
SC Chemistry; Materials Science
GA CQ0YE
UT WOS:000360323700041
ER
PT J
AU Mulavara, AP
Kofman, IS
De Dios, YE
Miller, C
Peters, BT
Goel, R
Galvan-Garza, R
Bloomberg, JJ
AF Mulavara, Ajitkumar P.
Kofman, Igor S.
De Dios, Yiri E.
Miller, Chris
Peters, Brian T.
Goel, Rahul
Galvan-Garza, Raquel
Bloomberg, Jacob J.
TI Using low levels of stochastic vestibular stimulation to improve
locomotor stability
SO FRONTIERS IN SYSTEMS NEUROSCIENCE
LA English
DT Article
DE stochastic resonance; balance control; vestibular stimulation;
stochastic electrical stimulation; body motion threshold; perceptual
motion threshold
ID FUNCTIONAL ANKLE INSTABILITY; APPLIED GALVANIC CURRENTS; ENHANCED
BALANCE CONTROL; HUMAN POSTURAL CONTROL; SENSORY SUBSTITUTION;
HAIR-CELLS; SENSORIMOTOR INTEGRATION; PARKINSONS-DISEASE; TACTILE
SENSATION; MOTILE RESPONSES
AB Low levels of bipolar binaural white noise based imperceptible stochastic electrical stimulation to the vestibular system (stochastic vestibular stimulation, SVS) have been shown to improve stability during balance tasks in normal, healthy subjects by facilitating enhanced information transfer using stochastic resonance (SR) principles. We hypothesize that detection of time-critical sub-threshold sensory signals using low levels of bipolar binaural SVS based on SR principles will help improve stability of walking during support surface perturbations. In the current study 13 healthy subjects were exposed to short continuous support surface perturbations for 60 s while walking on a treadmill and simultaneously viewing perceptually matched linear optic flow. Low levels of bipolar binaural white noise based SVS were applied to the vestibular organs. Multiple trials of the treadmill locomotion test were performed with stimulation current levels varying in the range of 0-1500 mu A, randomized across trials. The results show that subjects significantly improved their walking stability during support surface perturbations at stimulation levels with peak amplitude predominantly in the range of 100-500 mu A consistent with the SR phenomenon. Additionally, objective perceptual motion thresholds were measured separately as estimates of internal noise while subjects sat on a chair with their eyes closed and received 1 Hz bipolar binaural sinusoidal electrical stimuli. The optimal improvement in walking stability was achieved on average with peak stimulation amplitudes of approximately 35% of perceptual motion threshold. This study shows the effectiveness of using low imperceptible levels of SVS to improve dynamic stability during walking on a laterally oscillating treadmill via the SR phenomenon.
C1 [Mulavara, Ajitkumar P.] Univ Space Res Assoc, Houston, TX 77058 USA.
[Kofman, Igor S.; De Dios, Yiri E.; Miller, Chris; Peters, Brian T.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Goel, Rahul] Univ Houston, Houston, TX USA.
[Galvan-Garza, Raquel] MIT, Cambridge, MA 02139 USA.
[Bloomberg, Jacob J.] NASA, Johnson Space Ctr, Houston, TX USA.
RP Mulavara, AP (reprint author), Univ Space Res Assoc, 2101 NASA Pkwy,SK B272, Houston, TX 77058 USA.
EM ajitkumar.p.mulavara@nasa.gov
RI Goel, Rahul/C-4480-2016
OI Goel, Rahul/0000-0002-3516-6938
NR 90
TC 4
Z9 4
U1 1
U2 5
PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
SN 1662-5137
J9 FRONT SYST NEUROSCI
JI Front. Syst. Neurosci.
PD AUG 24
PY 2015
VL 9
AR 117
DI 10.3389/fnsys.2015.00117
PG 14
WC Neurosciences
SC Neurosciences & Neurology
GA CU9FU
UT WOS:000363850500001
PM 26347619
ER
PT J
AU Ruffle, PME
Kemper, F
Jones, OC
Sloan, GC
Kraemer, KE
Woods, PM
Boyer, ML
Srinivasan, S
Antoniou, V
Lagadec, E
Matsuura, M
McDonald, I
Oliveira, JM
Sargent, BA
Sewilo, M
Szczerba, R
van Loon, JT
Volk, K
Zijlstra, AA
AF Ruffle, Paul M. E.
Kemper, F.
Jones, O. C.
Sloan, G. C.
Kraemer, K. E.
Woods, Paul M.
Boyer, M. L.
Srinivasan, S.
Antoniou, V.
Lagadec, E.
Matsuura, M.
McDonald, I.
Oliveira, J. M.
Sargent, B. A.
Sewilo, M.
Szczerba, R.
van Loon, J. Th.
Volk, K.
Zijlstra, A. A.
TI Spitzer infrared spectrograph point source classification in the Small
Magellanic Cloud
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: spectroscopic; surveys; dust, extinction; H ii regions;
Magellanic Clouds; infrared: stars
ID GIANT BRANCH STARS; LONG-PERIOD VARIABLES; YOUNG STELLAR OBJECTS;
WOLF-RAYET STARS; SPACE-TELESCOPE OBSERVATIONS; BINARY HD 5980;
VLT-FLAMES SURVEY; ULTRAVIOLET INTERSTELLAR ABSORPTION;
SPECTROSCOPIC-EXPLORER OBSERVATIONS; EMISSION-LINE STARS
AB The Magellanic Clouds are uniquely placed to study the stellar contribution to dust emission. Individual stars can be resolved in these systems even in the mid-infrared, and they are close enough to allow detection of infrared excess caused by dust. We have searched the Spitzer Space Telescope data archive for all Infrared Spectrograph (IRS) staring-mode observations of the Small Magellanic Cloud (SMC) and found that 209 Infrared Array Camera (IRAC) point sources within the footprint of the Surveying the Agents of Galaxy Evolution in the Small Magellanic Cloud (SAGE-SMC) Spitzer Legacy programme were targeted, within a total of 311 staring-mode observations. We classify these point sources using a decision tree method of object classification, based on infrared spectral features, continuum and spectral energy distribution shape, bolometric luminosity, cluster membership and variability information. We find 58 asymptotic giant branch (AGB) stars, 51 young stellar objects, 4 post-AGB objects, 22 red supergiants, 27 stars (of which 23 are dusty OB stars), 24 planetary nebulae (PNe), 10 Wolf-Rayet stars, 3 H ii regions, 3 R Coronae Borealis stars, 1 Blue Supergiant and 6 other objects, including 2 foreground AGB stars. We use these classifications to evaluate the success of photometric classification methods reported in the literature.
C1 [Ruffle, Paul M. E.; Jones, O. C.; McDonald, I.; Zijlstra, A. A.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Ruffle, Paul M. E.; Kemper, F.; Srinivasan, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Jones, O. C.; Volk, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Kraemer, K. E.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA.
[Woods, Paul M.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Antoniou, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lagadec, E.] Univ Nice Sophia Antipolis, Lab Lagrange, CNRS, Observ Cote Azur, F-06304 Nice, France.
[Matsuura, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Matsuura, M.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Oliveira, J. M.; van Loon, J. Th.] Keele Univ, Lennard Jones Labs, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England.
[Sargent, B. A.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA.
[Sewilo, M.] Space Sci Inst, Boulder, CO 80301 USA.
[Sewilo, M.] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr 366, Baltimore, MD 21218 USA.
[Szczerba, R.] N Copernicus Astron Ctr, PL-87100 Torun, Poland.
EM ciska@asiaa.sinica.edu.tw
RI Woods, Paul/E-6926-2011; Kemper, Francisca/D-8688-2011; Antoniou,
Vallia/E-3837-2013;
OI Woods, Paul/0000-0003-4340-3590; Kemper, Francisca/0000-0003-2743-8240;
Antoniou, Vallia/0000-0001-7539-1593; Jones, Olivia/0000-0003-4870-5547;
Kraemer, Kathleen/0000-0002-2626-7155
FU STFC; National Science Council; Ministry of Science and Technology
[NSC100-2112-M-001-023-MY3, MOST103-2112-M-001-0330]; NASA ADP
[NNX11AB06G]; Polish NCN grant [2011/01/B/ST9/02031,
DEC-2013/08/M/ST9/00664]; National Aeronautics and Space Administration;
NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]
FX The authors wish to thank Paul Ruffle's partner Rose Wheeler, Rose
provided access to Paul's notes and files, which allowed us to finish
this work. PMER thanks Academia Sinica Institute of Astronomy and
Astrophysics (ASIAA) for their financial support and hospitality during
the preparation of this work. The authors thank David Whelan for making
available Spitzer spectra of point sources described in his 2013 paper.
Astrophysics at JBCA is supported by STFC. FK acknowledges support from
the former National Science Council and the Ministry of Science and
Technology in the form of grants NSC100-2112-M-001-023-MY3 and
MOST103-2112-M-001-0330. BAS acknowledges support from NASA ADP
NNX11AB06G. RSz acknowledges support from the Polish NCN grant
2011/01/B/ST9/02031. The research presented here was conducted within
the scope of the HECOLS International Associated Laboratory, supported
in part by the Polish NCN grant DEC-2013/08/M/ST9/00664 (E.L.; R.Sz).
This work is based (in part) on observations made with the Spitzer Space
Telescope, obtained from the NASA/IPAC Infrared Science Archive, both of
which are operated by the Jet Propulsion Laboratory, California
Institute of Technology under a contract with the National Aeronautics
and Space Administration. 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. 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 Hobble Space Telescope (HST) data is provided by the NASA
Office of Space Science via grant NNX13AC07G and by other grants and
contracts. This research has also made use of the SAGE CASJobs data
base, which made possible by the Sloan Digital Sky Survey Collaboration;
SAOImage DS9, developed by Smithsonian Astrophysical Observatory; the
VizieR catalogue access tool. CDS, Strasbourg, France; the SIMBAD data
base, operated at CDS, Strasbourg, France; and NASA's Astrophysics Data
System Bibliographic Services.
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JI Mon. Not. Roy. Astron. Soc.
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DI 10.1093/mnras/stv1106
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SC Astronomy & Astrophysics
GA CQ8HA
UT WOS:000360846400013
ER
PT J
AU Agius, NK
Alighieri, SD
Viaene, S
Baes, M
Sansom, AE
Bourne, N
Bland-Hawthorn, J
Brough, S
Davis, TA
De Looze, I
Driver, SP
Dunne, L
Dye, S
Eales, SA
Hughes, TM
Ivison, RJ
Kelvin, LS
Maddox, S
Mahajan, S
Pappalardo, C
Robotham, ASG
Rowlands, K
Temi, P
Valiante, E
AF Agius, N. K.
Alighieri, S. di Serego
Viaene, S.
Baes, M.
Sansom, A. E.
Bourne, N.
Bland-Hawthorn, J.
Brough, S.
Davis, T. A.
De Looze, I.
Driver, S. P.
Dunne, L.
Dye, S.
Eales, S. A.
Hughes, T. M.
Ivison, R. J.
Kelvin, L. S.
Maddox, S.
Mahajan, S.
Pappalardo, C.
Robotham, A. S. G.
Rowlands, K.
Temi, P.
Valiante, E.
TI H-ATLAS/GAMA and HeViCS - dusty early-type galaxies in different
environments
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: statistical; galaxies: elliptical and lenticular, cD; galaxies:
evolution; submillimetre: galaxies
ID HERSCHEL REFERENCE SURVEY; VIRGO CLUSTER SURVEY; MASS ASSEMBLY GAMA;
SCIENCE DEMONSTRATION PHASE; SPECTRAL ENERGY-DISTRIBUTIONS;
STAR-FORMATION RATE; ATLAS(3D) PROJECT; NEARBY GALAXIES; ELLIPTIC
GALAXIES; LOCAL UNIVERSE
AB The Herschel Space Observatory has had a tremendous impact on the study of extragalactic dust. Specifically, early-type galaxies (ETG) have been the focus of several studies. In this paper, we combine results from two Herschel studies - a Virgo cluster study Herschel Virgo Cluster Survey (HeViCS) and a broader, low-redshift Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS)/Galaxy and Mass Assembly (GAMA) study - and contrast the dust and associated properties for similar mass galaxies. This comparison is motivated by differences in results exhibited between multiple Herschel studies of ETG. A comparison between consistent modified blackbody derived dust mass is carried out, revealing strong differences between the two samples in both dust mass and dust-to-stellar mass ratio. In particular, the HeViCS sample lacks massive ETG with as high a specific dust content as found in H-ATLAS. This is most likely connected with the difference in environment for the two samples. We calculate nearest neighbour environment densities in a consistent way, showing that H-ATLAS ETG occupy sparser regions of the local Universe, whereas HeViCS ETG occupy dense regions. This is also true for ETG that are not Herschel-detected but are in the Virgo and GAMA parent samples. Spectral energy distributions are fit to the panchromatic data. From these, we find that in H-ATLAS the specific star formation rate anticorrelates with stellar mass and reaches values as high as in our Galaxy. On the other hand HeViCS ETG appear to have little star formation. Based on the trends found here, H-ATLAS ETG are thought to have more extended star formation histories and a younger stellar population than HeViCS ETG.
C1 [Agius, N. K.; Sansom, A. E.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Alighieri, S. di Serego] Ist Nazl Fis Nucl, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Viaene, S.; Baes, M.; De Looze, I.; Hughes, T. M.] Sterrunkundig Observ UGent, B-9000 Ghent, Belgium.
[Bourne, N.; Dunne, L.; Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Bland-Hawthorn, J.] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Brough, S.] Australian Astron Observ, N Ryde, NSW 1670, Australia.
[Davis, T. A.; Ivison, R. J.] European Southern Observ, D-85748 Garching, Germany.
[De Looze, I.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Driver, S. P.; Kelvin, L. S.; Robotham, A. S. G.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia.
[Driver, S. P.; Kelvin, L. S.; Robotham, A. S. G.; Rowlands, K.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Dunne, L.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand.
[Dye, S.; Maddox, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Eales, S. A.; Valiante, E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales.
[Kelvin, L. S.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Mahajan, S.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia.
[Pappalardo, C.] Univ Lisbon, Observ Astron Lisboa, CAAUL, P-1349018 Lisbon, Portugal.
[Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
RP Agius, NK (reprint author), Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
EM aesansom@uclan.ac.uk
RI Ivison, R./G-4450-2011;
OI Ivison, R./0000-0001-5118-1313; Maddox, Stephen/0000-0001-5549-195X;
Davis, Timothy/0000-0003-4932-9379; Robotham, Aaron/0000-0003-0429-3579;
Dye, Simon/0000-0002-1318-8343; di Serego Alighieri,
Sperello/0000-0001-8769-2692
FU Science and Technology Facilities Council; European Research Council;
Flemish Fund for Scientific Research (FWO-Vlaanderen); STFC (UK); ARC
(Australia); AAO
FX We would like to acknowledge and thank Elisabete da Cunha for her
contribution of modified MAGPHYS libraries. NKA acknowledges the support
of the Science and Technology Facilities Council. LD, RH and SJM
acknowledge support from the European Research Council Advanced Grant
COSMICISM. IDL gratefully acknowledges the support of the Flemish Fund
for Scientific Research (FWO-Vlaanderen). KR acknowledges support from
the European Research Council Starting Grant SEDmorph (P.I. V. Wild).
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 web site is http://www.h-atlas.org/. GAMA is a joint European
Australasian project based around a spectroscopic campaign using the
AAT. The GAMA input catalogue is based on data taken from the SDSS and
UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA
regions is being obtained by a number of independent survey programmes
including GALEX MIS, VST KIDS, VISTA VIKING, WISE, Herschel-ATLAS. GMRT
and ASKAP providing UV to radio coverage. GAMA is funded by the STFC
(UK), the ARC (Australia), the AAO, and the participating institutions.
The GAMA web site is http://www.gamma-survey.org/. We thank Gianfranco
De Zotti and Michal Michalowski for helpful comments on an earlier draft
of this paper. Thanks to the anonymous referee for useful suggestions
that improved the paper.
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JI Mon. Not. Roy. Astron. Soc.
PD AUG 21
PY 2015
VL 451
IS 4
BP 3815
EP 3835
DI 10.1093/mnras/stv1191
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8HA
UT WOS:000360846400033
ER
PT J
AU Curran, PA
Miller-Jones, JCA
Rushton, AP
Pawar, DD
Anderson, GE
Altamirano, D
Krimm, HA
Broderick, JW
Belloni, TM
Fender, RP
Kording, EG
Maitra, D
Markoff, S
Migliari, S
Rumsey, C
Rupen, MP
Russell, DM
Russell, TD
Sarazin, CL
Sivakoff, GR
Soria, R
Tetarenko, AJ
Titterington, D
Tudose, V
AF Curran, P. A.
Miller-Jones, J. C. A.
Rushton, A. P.
Pawar, D. D.
Anderson, G. E.
Altamirano, D.
Krimm, H. A.
Broderick, J. W.
Belloni, T. M.
Fender, R. P.
Kording, E. G.
Maitra, D.
Markoff, S.
Migliari, S.
Rumsey, C.
Rupen, M. P.
Russell, D. M.
Russell, T. D.
Sarazin, C. L.
Sivakoff, G. R.
Soria, R.
Tetarenko, A. J.
Titterington, D.
Tudose, V.
TI Radio polarimetry as a probe of unresolved jets: the 2013 outburst of
XTE J1908+094
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: close; stars: individual: XTE J1908+094; X-rays: binaries;
X-rays: bursts
ID BLACK-HOLE CANDIDATE; X-RAY BINARIES; ARCMINUTE MICROKELVIN IMAGER; GX
339-4; HARD STATE; TIMING BEHAVIOR; MAXI J1659-152; MAGNETIC-FIELD;
LOW/HARD STATE; SKY SURVEY
AB XTE J1908+094 is an X-ray transient black hole candidate in the Galactic plane that was observed in outburst in 2002 and 2013. Here we present multifrequency radio and X-ray data, including radio polarimetry, spanning the entire period of the 2013 outburst. We find that the X-ray behaviour of XTE J1908+094 traces the standard black hole hardness-intensity path, evolving from a hard state, through a soft state, before returning to a hard state and quiescence. Its radio behaviour is typical of a compact jet that becomes quenched before discrete ejecta are launched during the late stages of X-ray softening. The radio and X-ray fluxes, as well as the light-curve morphologies, are consistent with those observed during the 2002 outburst of this source. The polarization angle during the rise of the outburst infers a jet orientation in agreement with resolved observations but also displays a gradual drift, which we associate with observed changes in the structure of the discrete ejecta. We also observe an unexpected 90A degrees rotation of the polarization angle associated with a second component.
C1 [Curran, P. A.; Miller-Jones, J. C. A.; Russell, T. D.; Soria, R.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Rushton, A. P.; Anderson, G. E.; Broderick, J. W.; Fender, R. P.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Rushton, A. P.; Altamirano, D.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Pawar, D. D.] RJ Coll, Dept Phys, Bombay 400086, Maharashtra, India.
[Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Krimm, H. A.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Belloni, T. M.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Kording, E. G.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Maitra, D.] Wheaton Coll, Dept Phys & Astron, Norton, MA 02766 USA.
[Markoff, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Migliari, S.] ESAC ESA, XMM Newton Sci Operat Ctr, E-28691 Madrid, Spain.
[Migliari, S.] Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain.
[Migliari, S.] Univ Barcelona, ICCUB, E-08028 Barcelona, Spain.
[Rumsey, C.; Titterington, D.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
[Rupen, M. P.] Natl Res Council Canada, Herzberg Astron & Astrophys, Penticton, BC V2A 6J9, Canada.
[Russell, D. M.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates.
[Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Sivakoff, G. R.; Tetarenko, A. J.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Tudose, V.] Inst Space Sci, RO-077125 Bucharest, Romania.
RP Curran, PA (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia.
EM peter.curran@curtin.edu.au
RI Miller-Jones, James/B-2411-2013; Sivakoff, Gregory/G-9602-2011; Tudose,
Valeriu/F-8976-2010;
OI Miller-Jones, James/0000-0003-3124-2814; Sivakoff,
Gregory/0000-0001-6682-916X; Russell, David/0000-0002-3500-631X;
Russell, Thomas/0000-0001-6958-8891; Anderson, Gemma/0000-0001-6544-8007
FU Australian Research Council [DP120102393]; Royal Society; NSERC; Spanish
Ministerio de Ciencia e Innovacion [AYA2013-47447-C03-1-P]; European
Research Council [267697]
FX We thank the anonymous referee for constructise comments. We also thank
T. J. Maccarone for useful discussions and A. Scaife for valuable input
on the AMI-LA data. This work was supported by Australian Research
Council grant DP120102393. DA acknowledges support from the Royal
Society. GRS is supported in part by an NSERC Discovery Grant. SM is
supported by the Spanish Ministerio de Ciencia e Innovacion (grant
AYA2013-47447-C03-1-P). This work was also supported in part by European
Research Council Advanced Grant 267697 '4 Pi Sky: Extreme Astrophysics
with Revolutionary Radio Telescopes'. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc, We thank
the staff of the Milliard Radio Astronomy Observatory for their
invaluable assistance in the operation of AMI-LA. LOFAR, the
Low-Frequency Array designed and constructed by ASTRON, has facilities
in several countries, that are owned by various parties (each with their
own funding sources), and that are collectively operated by the
International LOFAR Telescope (ILT) foundation under a joint scientific
policy. This research has made use of NASA's Astrophysics Data System.
Swift/XRT data were supplied by the UK Swift Science Data Centre at the
University of Leicester, and Swift/BAT transient monitor results were
provided by the Swift/BAT team.
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DI 10.1093/mnras/stv1252
PG 11
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SC Astronomy & Astrophysics
GA CQ8HA
UT WOS:000360846400045
ER
PT J
AU Gofford, J
Reeves, JN
McLaughlin, DE
Braito, V
Turner, TJ
Tombesi, F
Cappi, M
AF Gofford, J.
Reeves, J. N.
McLaughlin, D. E.
Braito, V.
Turner, T. J.
Tombesi, F.
Cappi, M.
TI The Suzaku view of highly ionized outflows in AGN - II. Location,
energetics and scalings with bolometric luminosity
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE line: identification; galaxies: active; galaxies: nuclei; X-rays:
galaxies
ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; ULTRA-FAST OUTFLOWS;
X-RAY-SPECTRUM; ACCRETION DISC OUTFLOWS; QUASAR APM 08279+5255;
RADIO-QUIET AGNS; ENERGY-DISTRIBUTIONS; ABSORPTION-LINES; WARM ABSORBERS
AB Ongoing studies with XMM-Newton have shown that powerful accretion disc winds, as revealed through highly ionized Fe K-shell absorption at E a parts per thousand yen 6.7 keV, are present in a significant fraction of active galactic nuclei (AGNs) in the local Universe (Tombesi et al. 2010a). In Gofford et al., we analysed a sample of 51 Suzaku-observed AGNs and independently detected Fe K absorption in similar to 40 per cent of the sample, and we measured the properties of the absorbing gas. In this work, we build upon these results to consider the properties of the associated wind. On average, the fast winds (v(w) > 0.01c) are located aEuroraEuro parts per thousand similar to 10(15-18) cm (typically similar to 10(2-4) r(s)) from their black hole, their mass outflow rates are of the order of and kinetic power is constrained to aEuroL(w)aEuro parts per thousand similar to 10(43-45) erg s(-1), equivalent to similar to(0.1-10 per cent)L-Edd. We find a fundamental correlation between the source bolometric luminosity and the wind velocity, with (90 per cent confidence), which indicates that more luminous AGN tend to harbour faster Fe K winds. The mass outflow rate of the winds are also consequently correlated with L-bol, such that more massive and more energetic winds are present in more luminous AGN. We investigate these properties in the framework of a continuum-driven wind, showing that the observed relationships are broadly consistent with a wind being accelerated by continuum-scattering. We find that, globally, a significant fraction (similar to 85 per cent) of the sample can plausibly exceed the L-w/L-bol similar to 0.5 per cent threshold thought necessary for feedback, while 45 per cent may also exceed the less conservative similar to 5 per cent of L-bol threshold as well. This suggests that the winds may be energetically significant for AGN-host-galaxy feedback processes.
C1 [Gofford, J.; Reeves, J. N.; Turner, T. J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Gofford, J.; Reeves, J. N.; McLaughlin, D. E.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Braito, V.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Tombesi, F.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Tombesi, F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Cappi, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
RP Gofford, J (reprint author), Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
EM jason.a.gofford@gmail.com
RI XRAY, SUZAKU/A-1808-2009;
OI Braito, Valentina/0000-0002-2629-4989; Cappi,
Massimo/0000-0001-6966-8920
FU ASI/INAF [I/037/12/0]; PRIN INAF; National Aeronautics and Space
Administration (NASA) [NNX12AH40G]
FX MC acknowledges support from contracts ASI/INAF no. I/037/12/0 and PRIN
INAF 2012. FT acknowledges support for this work by the National
Aeronautics and Space Administration (NASA) under grant no NNX12AH40G
issued through the Astrophysics Data Analysis Program, part of the ROSES
2010.
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BP 4169
EP 4182
DI 10.1093/mnras/stv1207
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8HA
UT WOS:000360846400062
ER
PT J
AU Desjaeques, V
Chluba, J
Silk, J
de Bernardis, F
Dore, O
AF Desjaeques, Vincent
Chluba, Jens
Silk, Joseph
de Bernardis, Francesco
Dore, Olivier
TI Detecting the cosmological recombination signal from space
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE cosmology: theory; early Universe
ID MICROWAVE BACKGROUND SPECTRUM; HALO OCCUPATION DISTRIBUTION;
STAR-FORMING GALAXIES; HYDROGEN RECOMBINATION; POWER SPECTRUM;
DARK-MATTER; RAYLEIGH-SCATTERING; ENERGY-SPECTRUM; THERMAL HISTORY;
SOUTH-POLE
AB Spectral distortions of the cosmic microwave background (CMB) have recently experienced an increased interest. One of the inevitable distortion signals of our cosmological concordance model is created by the cosmological recombination process, just a little before photons last scatter at redshift "yes">z a parts per thousand integral 1100. These cosmological recombination lines, emitted by the hydrogen and helium plasma, should still be observable as tiny deviation from the CMB blackbody spectrum in the cm-dm spectral bands. In this paper, we present a forecast for the detectability of the recombination signal with future satellite experiments. We argue that serious consideration for future CMB experiments in space should be given to probing spectral distortions and, in particular, the recombination line signals. The cosmological recombination radiation not only allows determination of standard cosmological parameters, but also provides a direct observational confirmation for one of the key ingredients of our cosmological model: the cosmological recombination history. We show that, with present technology, such experiments are futuristic but feasible. The potential rewards won by opening this new window to the very early universe could be considerable.
C1 [Desjaeques, Vincent] Univ Geneva, Dept Phys Theor, CH-1211 Geneva, Switzerland.
[Desjaeques, Vincent] Univ Geneva, CAP, CH-1211 Geneva, Switzerland.
[Chluba, Jens] Kav1i Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
[Chluba, Jens; Silk, Joseph] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Silk, Joseph] CNRS, F-75014 Paris, France.
[Silk, Joseph] UPMC, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Silk, Joseph] Univ Paris Diderot, CNRS, CEA DSM IRFU, Lab AlM Paris Saclay, F-91191 Gif Sur Yvette, France.
[de Bernardis, Francesco] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dore, Olivier] CALTECH, Pasadena, CA 91109 USA.
RP Desjaeques, V (reprint author), Univ Geneva, Dept Phys Theor, 24 Quai Ernest Ansermer, CH-1211 Geneva, Switzerland.
EM Vincerit.Desjacques@unige.ch
OI Chluba, Jens/0000-0003-3725-6096
FU Swiss National Science Foundation; Royal Society
FX VD would like to thank Marco Tucci for discussions, and acknowledges
support by the Swiss National Science Foundation. IS acknowledges
discussions with S. Colafrancesco. JC is supported by the Royal Society
as a Royal Society University Research Fellow at the University of
Cambridge, UK. 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.
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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 AUG 21
PY 2015
VL 451
IS 4
BP 4460
EP 4470
DI 10.1093/mnras/stv1291
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8HA
UT WOS:000360846400086
ER
PT J
AU Fortenberry, RC
Yu, Q
Mancini, JS
Bowman, JM
Lee, TJ
Crawford, TD
Klemperer, WF
Francisco, JS
AF Fortenberry, Ryan C.
Yu, Qi
Mancini, John S.
Bowman, Joel M.
Lee, Timothy J.
Crawford, T. Daniel
Klemperer, William F.
Francisco, Joseph S.
TI Communication: Spectroscopic consequences of proton delocalization in
OCHCO+
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID QUARTIC FORCE-FIELDS; VIBRATIONAL FREQUENCIES; ANALYTIC EVALUATION;
ENERGY GRADIENTS; BASIS-SETS; CHEMISTRY; MOLECULES; HCO+; ISOTOPOLOGUES;
COMPLEXES
AB Even though quartic force fields (QFFs) and highly accurate coupled cluster computations describe the OCHCO+ cation at equilibrium as a complex between carbon monoxide and the formyl cation, two notable and typical interstellar and atmospheric molecules, the prediction from the present study is that the equilibrium C-infinity v structure is less relevant to observables than the saddle-point D-infinity h structure. This is the conclusion from diffusion Monte Carlo and vibrational self-consistent field/virtual state configuration interaction calculations utilizing a semi-global potential energy surface. These calculations demonstrate that the proton "rattle" motion (nu(6)) has centrosymmetric delocalization of the proton over the D-infinity h barrier lying only 393.6 cm(-1) above the double-well OCHCO+ C-infinity v minima. As a result, this molecule will likely appear D-infinity h, and the rotational spectrum will be significantly dimmer than the computed equilibrium 2.975 D center-of-mass dipole moment indicates. However, the proton transfer fundamental, determined to be at roughly 300 cm(-1), has a very strong intensity. This prediction as well as those of other fundamentals should provide useful guides for laboratory detection of this cation. Finally, it is shown that the two highest energy QFF-determined modes are actually in good agreement with their vibrational configuration interaction counterparts. These high-level quantum chemical methods provide novel insights into this fascinating and potentially common interstellar molecule. (C) 2015 AIP Publishing LLC.
C1 [Fortenberry, Ryan C.] Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA.
[Yu, Qi; Mancini, John S.; Bowman, Joel M.] Emory Univ, Dept Chem, Atlanta, GA 30322 USA.
[Yu, Qi; Mancini, John S.; Bowman, Joel M.] Emory Univ, Cherry L Emerson Ctr Sci Computat, Atlanta, GA 30322 USA.
[Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, Moffett Field, CA 94035 USA.
[Crawford, T. Daniel] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA.
[Klemperer, William F.] Harvard Univ, Dept Chem, Cambridge, MA 02138 USA.
[Francisco, Joseph S.] Univ Nebraska, Dept Chem, Lincoln, NE 68588 USA.
RP Fortenberry, RC (reprint author), Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA.
EM rfortenberry@georgiasouthern.edu; jmbowma@emory.edu
RI Lee, Timothy/K-2838-2012; Crawford, Thomas/A-9271-2017
OI Crawford, Thomas/0000-0002-7961-7016
FU Georgia Southern University; U.S. National Science Foundation (NSF)
[CHE-1463552]; NSF [CHE-1058420, CHE-0741927]; National Aeronautics and
Space Administration through the NASA Astrobiology Institute through the
Science Mission Directorate [NNH13ZDA017C]
FX R.C.F. thanks Georgia Southern University for start-up funds utilized in
this effort. The U.S. National Science Foundation (NSF) Grant No.
CHE-1463552 supported the work done by J. M. B., Q. Y., and J. S. M. T.
D. C. acknowledges NSF Award Nos. CHE-1058420 and CHE-0741927. Support
also comes from the National Aeronautics and Space Administration
through the NASA Astrobiology Institute under Cooperative Agreement
Notice No. NNH13ZDA017C issued through the Science Mission Directorate.
T. J. L. and R. C. F. also acknowledge Dr. Xinchuan Huang of the SETI
Institute for useful discussions.
NR 45
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Z9 10
U1 2
U2 17
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-9606
EI 1089-7690
J9 J CHEM PHYS
JI J. Chem. Phys.
PD AUG 21
PY 2015
VL 143
IS 7
AR 071102
DI 10.1063/1.4929345
PG 5
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA CQ2OJ
UT WOS:000360440400002
PM 26298107
ER
PT J
AU Goel, R
Kofman, I
Jeevarajan, J
De Dios, Y
Cohen, HS
Bloomberg, JJ
Mulavara, AP
AF Goel, Rahul
Kofman, Igor
Jeevarajan, Jerome
De Dios, Yiri
Cohen, Helen S.
Bloomberg, Jacob J.
Mulavara, Ajitkumar P.
TI Using Low Levels of Stochastic Vestibular Stimulation to Improve Balance
Function
SO PLOS ONE
LA English
DT Article
ID APPLIED GALVANIC CURRENTS; HUMAN POSTURAL CONTROL; HAIR-CELLS;
SENSORIMOTOR INTEGRATION; PARKINSONS-DISEASE; MOTILE RESPONSES;
SQUIRREL-MONKEY; NERVE AFFERENTS; NOISE; RESONANCE
AB Low-level stochastic vestibular stimulation (SVS) has been associated with improved postural responses in the medio-lateral (ML) direction, but its effect in improving balance function in both the ML and anterior-posterior (AP) directions has not been studied. In this series of studies, the efficacy of applying low amplitude SVS in 0-30 Hz range between the mastoids in the ML direction on improving cross-planar balance function was investigated. Forty-five (45) subjects stood on a compliant surface with their eyes closed and were instructed to maintain a stable upright stance. Measures of stability of the head, trunk, and whole body were quantified in ML, AP and combined APML directions. Results show that binaural bipolar SVS given in the ML direction significantly improved balance performance with the peak of optimal stimulus amplitude predominantly in the range of 100-500 mu A for all the three directions, exhibiting stochastic resonance (SR) phenomenon. Objective perceptual and body motion thresholds as estimates of internal noise while subjects sat on a chair with their eyes closed and were given 1 Hz bipolar binaural sinusoidal electrical stimuli were also measured. In general, there was no significant difference between estimates of perceptual and body motion thresholds. The average optimal SVS amplitude that improved balance performance (peak SVS amplitude normalized to perceptual threshold) was estimated to be 46% in ML, 53% in AP, and 50% in APML directions. A miniature patch-type SVS device may be useful to improve balance function in people with disabilities due to aging, Parkinson's disease or in astronauts returning from long-duration space flight.
C1 [Goel, Rahul] Univ Houston, Dept Hlth & Human Performance, Houston, TX USA.
[Kofman, Igor; De Dios, Yiri] Wyle Sci, Technol & Engn Grp, Houston, TX USA.
[Jeevarajan, Jerome; Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Neurosci Lab, Houston, TX 77058 USA.
[Cohen, Helen S.] Baylor Coll Med, Dept Otolaryngol Head & Neck Surg, Houston, TX 77030 USA.
[Mulavara, Ajitkumar P.] Univ Space Res Assoc, Houston, TX 77058 USA.
RP Mulavara, AP (reprint author), Univ Space Res Assoc, Houston, TX 77058 USA.
EM ajitkumar.p.mulavara@nasa.gov
RI Goel, Rahul/C-4480-2016
OI Goel, Rahul/0000-0002-3516-6938
FU National Space Biomedical Research Institute through NASA [NCC 9-58-SA
02801]; NASA [NCC 9-58-SA 02001]; National Institute of Health
[RO1-DC009031]; Wyle Science, Technology and Engineering Group
FX This study was supported in part by a grant from the National Space
Biomedical Research Institute through NASA NCC 9-58-SA 02801 to Jacob
Bloomberg, NASA NCC 9-58-SA 02001 to Ajitkumar Mulavara and by a grant
from the National Institute of Health through RO1-DC009031 to Helen
Cohen. The funders had no role in study design, data collection and
analysis, decision to publish, or preparation of the manuscript. Wyle
Science, Technology and Engineering Group provided support in the form
of salaries for authors IK and YD but did not have any additional role
in the study design, data collection and analysis, decision to publish,
or preparation of the manuscript. The specific roles of these authors
are articulated in the 'author contributions' section.
NR 53
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U1 0
U2 6
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 AUG 21
PY 2015
VL 10
IS 8
AR e0136335
DI 10.1371/journal.pone.0136335
PG 24
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CP5MR
UT WOS:000359926900102
PM 26295807
ER
PT J
AU Corcoran, MF
Nichols, JS
Pablo, H
Shenar, T
Pollock, AMT
Waldron, WL
Moffat, AFJ
Richardson, ND
Russell, CMP
Hamaguchi, K
Huenemoerder, DP
Oskinova, L
Hamann, WR
Naze, Y
Ignace, R
Evans, NR
Lomax, JR
Hoffman, JL
Gayley, K
Owocki, SP
Leutenegger, M
Gull, TR
Hole, KT
Lauer, J
Iping, RC
AF Corcoran, M. F.
Nichols, J. S.
Pablo, H.
Shenar, T.
Pollock, A. M. T.
Waldron, W. L.
Moffat, A. F. J.
Richardson, N. D.
Russell, C. M. P.
Hamaguchi, K.
Huenemoerder, D. P.
Oskinova, L.
Hamann, W. -R.
Naze, Y.
Ignace, R.
Evans, N. R.
Lomax, J. R.
Hoffman, J. L.
Gayley, K.
Owocki, S. P.
Leutenegger, M.
Gull, T. R.
Hole, K. T.
Lauer, J.
Iping, R. C.
TI A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE
ECLIPSING BINARY, delta ORIONIS Aa. I. OVERVIEW OF THE X-RAY SPECTRUM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; binaries: eclipsing; stars: early-type; stars:
individual (Delta Ori); stars: mass-loss; X-rays: stars
ID HOT-STAR WINDS; O-TYPE STARS; RADIATION-DRIVEN WINDS; COLLIDING WINDS;
EMISSION; CHANDRA; SPECTROSCOPY; SIMULATIONS; SYSTEMS; MODELS
AB We present an overview of four deep phase-constrained Chandra HETGS X-ray observations of delta Ori A. Delta Ori A is actually a triple system that includes the nearest massive eclipsing spectroscopic binary, delta Ori Aa, the only such object that can be observed with little phase-smearing with the Chandra gratings. Since the fainter star, delta Ori Aa2, has a much lower X-ray luminosity than the brighter primary (delta Ori Aa1), delta Ori Aa provides a unique system with which to test the spatial distribution of the X-ray emitting gas around delta Ori Aa1 via occultation by the photosphere of, and wind cavity around, the X-ray dark secondary. Here we discuss the X-ray spectrum and X-ray line profiles for the combined observation, having an exposure time of nearly 500 ks and covering nearly the entire binary orbit. The companion papers discuss the X-ray variability seen in the Chandra spectra, present new space-based photometry and ground-based radial velocities obtained simultaneously with the X-ray data to better constrain the system parameters, and model the effects of X-rays on the optical and UV spectra. We find that the X-ray emission is dominated by embedded wind shock emission from star Aa1, with little contribution from the tertiary star Ab or the shocked gas produced by the collision of the wind of Aa1 against the surface of Aa2. We find a similar temperature distribution to previous X-ray spectrum analyses. We also show that the line half-widths are about 0.3-0.5 times the terminal velocity of the wind of star Aa1. We find a strong anti-correlation between line widths and the line excitation energy, which suggests that longer-wavelength, lower-temperature lines form farther out in the wind. Our analysis also indicates that the ratio of the intensities of the strong and weak lines of Fe XVII and Ne X are inconsistent with model predictions, which may be an effect of resonance scattering.
C1 [Corcoran, M. F.; Hamaguchi, K.; Leutenegger, M.; Iping, R. C.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Corcoran, M. F.; Hamaguchi, K.; Leutenegger, M.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Nichols, J. S.; Lauer, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pablo, H.; Moffat, A. F. J.; Richardson, N. D.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Pablo, H.; Moffat, A. F. J.; Richardson, N. D.] Univ Montreal, CRAQ, Montreal, PQ H3C 3J7, Canada.
[Shenar, T.; Oskinova, L.; Hamann, W. -R.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Pollock, A. M. T.] European Space Agcy, XMM Newton Sci Operat Ctr, European Space Astron Ctr, E-28691 Villanueva De La Canada, Spain.
[Waldron, W. L.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Russell, C. M. P.] NASA GSFC, Greenbelt, MD 20771 USA.
[Hamaguchi, K.; Leutenegger, M.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Huenemoerder, D. P.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Naze, Y.] Univ Liege, Grp Astrophys Hautes Energies, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium.
[Ignace, R.] E Tennessee State Univ, Phys & Astron, Johnson City, TN 37614 USA.
[Evans, N. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lomax, J. R.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Hoffman, J. L.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Gayley, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Owocki, S. P.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Gull, T. R.] NASA Goddard Space Flight Ctr, Lab Extraterr Planets & Stellar Astrophys, Greenbelt, MD 20771 USA.
[Hole, K. T.] Weber State Univ, Dept Phys, Ogden, UT 84408 USA.
[Iping, R. C.] NASA Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Iping, R. C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Corcoran, MF (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
EM michael.f.corcoran@nasa.gov
FU National Aeronautics and Space Administration [GO3-14015A, GO3-14015E];
National Aeronautics Space Administration [NAS8-03060]; NASA
[NNG06EO90A, NNX13AF40G]; Chandra X-ray Center NASA [NAS8-03060]; NASA
Postdoctoral Program at the Goddard Space Flight Center; Leibniz
Graduate School for Quantitative Spectroscopy in Astrophysics; Leibniz
Institute for Astrophysics Potsdam (AIP); institute of Physics and
Astronomy of the University of Potsdam; Fonds National de la Recherche
Scientifique (Belgium); Communaute Francaise de Belgique; PRODEX XMM and
Integral contracts; "Action de Recherche Concertee" (CFWB-Academie
Wallonie Europe); CRAQ (Centre de Recherche en Astrophysique du Quebec)
fellowship; NSERC (Canada); FRQNT (Quebec); NSF [AST-0807477]
FX We thank the MOST team for the award of observing time for delta Ori A.
We also thank our anonymous referee, whose comments significantly
improved this paper. M.F.C. thanks John Houck and Michael Nowak for many
helpful discussions concerning data analysis with ISIS. Support for this
work was provided by the National Aeronautics and Space Administration
through Chandra Award Number GO3-14015A and GO3-14015E issued by the
Chandra X-ray Observatory Center, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of the National Aeronautics
Space Administration under contract NAS8-03060. M.F.C., J.S.N., W.L.W.,
C.M.P.R., and K.H. gratefully acknowledge this support. M.F.C.
acknowledges support from NASA under cooperative agreement number
NNG06EO90A. N.R.E. is grateful for support from the Chandra X-ray Center
NASA Contract NAS8-03060. C.M.P.R. is supported by an appointment to the
NASA Postdoctoral Program at the Goddard Space Flight Center,
administered by Oak Ridge Associated Universities through a contract
with NASA. T.S. is grateful for financial support from the Leibniz
Graduate School for Quantitative Spectroscopy in Astrophysics, a joint
project of the Leibniz Institute for Astrophysics Potsdam (AIP) and the
institute of Physics and Astronomy of the University of Potsdam. Y.N.
acknowledges support from the Fonds National de la Recherche
Scientifique (Belgium), the Communaute Francaise de Belgique, the PRODEX
XMM and Integral contracts, and the "Action de Recherche Concertee"
(CFWB-Academie Wallonie Europe). N.D.R. gratefully acknowledges his CRAQ
(Centre de Recherche en Astrophysique du Quebec) fellowship. A.F.J.M. is
grateful for financial support from NSERC (Canada) and FRQNT (Quebec).
J.L.H. acknowledges support from NASA award NNX13AF40G and NSF award
AST-0807477. This research has made use of NASA's Astrophysics Data
System. This research has made use of data and/or software provided by
the High Energy Astrophysics Science Archive Research Center (HEASARC),
which is a service of the Astrophysics Science Division at NASA/GSFC and
the High Energy Astrophysics Division of the Smithsonian Astrophysical
Observatory. This research also made use of the Chandra Transmission
Grating Catalog and archive (http://tgcat.mit.edu). The SPH simulations
presented in this paper made use of the resources provided by the NASA
High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center.
NR 68
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Z9 4
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2015
VL 809
IS 2
AR 132
DI 10.1088/0004-637X/809/2/132
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9EC
UT WOS:000361655100025
ER
PT J
AU Dotson, A
Georganopoulos, M
Meyer, ET
McCann, K
AF Dotson, Amanda
Georganopoulos, Markos
Meyer, Eileen T.
McCann, Kevin
TI ON THE LOCATION OF THE 2009 GEV FLARES OF BLAZAR PKS 1510-089
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; gamma rays: galaxies; quasars: individual (PKS
1510-089); radiation mechanisms: non-thermal
ID ACTIVE GALACTIC NUCLEI; GAMMA-RAY VARIABILITY; 3C 454.3; MULTIWAVELENGTH
OBSERVATIONS; FLARING ACTIVITY; EMISSION-LINE; FERMI BLAZARS; INNER JET;
QUASAR; RADIATION
AB Most of the radiated power of blazars is produced at GeV energies via inverse Compton scattering at an unknown distance from the central engine. Possible seed photon sources map to different locations along the jet spanning two orders of magnitude in distance from the black hole, ranging from the broad-line region (BLR, similar to 0.1 pc), to the molecular torus (MT, similar to 1-few pc), to the very long baseline interferometry (VLBI) radio core zone at similar to 10 pc. Here, we apply a diagnostic for identifying the GeV emission zone (GEZ) in blazar PKS 1510-089 using four bright gamma-ray flares detected by Fermi in 2009. As shown by Dotson et al., the flare decay time should be energy-independent for flares in the BLR, but faster at higher energies for flares in the MT. We find that in the two cases where the gamma-ray flare was not accompanied by an optical flare, the decay times show an energydependence suggesting a location in the MT. For the two GeV flares accompanied by optical flares, we obtained very fast decay times (less than or similar to 3 hr) in both low and high energy Fermi bands. For these flares, considering the simultaneous > 100 GeV detection by HESS (H. E. S. S. Collaboration et al.) and the ejection of a superluminal component from the VLBI radio core in one case, our results suggest that both flares came from the vicinity of the VLBI core. We thus suggest that the GEZ is spread over a wide range of locations beyond the BLR.
C1 [Dotson, Amanda; Georganopoulos, Markos; Meyer, Eileen T.; McCann, Kevin] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Georganopoulos, Markos] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Meyer, Eileen T.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Dotson, A (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
OI Meyer, Eileen/0000-0002-7676-9962
FU Fermi grant [NNX14AQ71G]
FX A.D. and M.G. acknowledge support from Fermi grant NNX14AQ71G.
NR 39
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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 AUG 20
PY 2015
VL 809
IS 2
AR 164
DI 10.1088/0004-637X/809/2/164
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9EC
UT WOS:000361655100057
ER
PT J
AU Gurnett, DA
Kurth, WS
Stone, EC
Cummings, AC
Krimigis, SM
Decker, RB
Ness, NF
Burlaga, LF
AF Gurnett, D. A.
Kurth, W. S.
Stone, E. C.
Cummings, A. C.
Krimigis, S. M.
Decker, R. B.
Ness, N. F.
Burlaga, L. F.
TI PRECURSORS TO INTERSTELLAR SHOCKS OF SOLAR ORIGIN
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; local interstellar matter; shock waves; Sun: heliosphere
ID GALACTIC COSMIC-RAYS; EARTHS BOW SHOCK; VOYAGER 1; RADIO EMISSIONS;
MAGNETIC-FIELDS; TERRESTRIAL FORESHOCK; TERMINATION SHOCK; PLASMA-WAVES;
HELIOPAUSE; FREQUENCY
AB On or about 2012 August 25, the Voyager 1 spacecraft crossed the heliopause into the nearby interstellar plasma. In the nearly three years that the spacecraft has been in interstellar space, three notable particle and field disturbances have been observed, each apparently associated with a shock wave propagating outward from the Sun. Here, we present a detailed analysis of the third and most impressive of these disturbances, with brief comparisons to the two previous events, both of which have been previously reported. The shock responsible for the third event was first detected on 2014 February 17 by the onset of narrowband radio emissions from the approaching shock, followed on 2014 May 13 by the abrupt appearance of intense electron plasma oscillations generated by electrons streaming outward ahead of the shock. Finally, the shock arrived on 2014 August 25, as indicated by a jump in the magnetic field strength and the plasma density. Various disturbances in the intensity and anisotropy of galactic cosmic rays were also observed ahead of the shock, some of which are believed to be caused by the reflection and acceleration of cosmic rays by the magnetic field jump at the shock, and/or by interactions with upstream plasma waves. Comparisons to the two previous weaker events show somewhat similar precursor effects, although differing in certain details. Many of these effects are very similar to those observed in the region called the "foreshock" that occurs upstream of planetary bow shocks, only on a vastly larger spatial scale.
C1 [Gurnett, D. A.; Kurth, W. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Stone, E. C.; Cummings, A. C.] CALTECH, Pasadena, CA 91125 USA.
[Krimigis, S. M.; Decker, R. B.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Ness, N. F.] Catholic Univ Amer, Washington, DC 20064 USA.
[Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gurnett, DA (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
EM donald-gurnett@uiowa.edu
OI Kurth, William/0000-0002-5471-6202
FU NASA [1279980, NNN12AA012, NNX12AC63G, NNG14PN24P]; Voyager Interstellar
Mission under NASA [NNN06AA01C]
FX The research at the University of Iowa was supported by NASA through
contract 1279980 with JPL. The research at Caltech was supported by NASA
contract NNN12AA012, and the research at the Johns Hopkins Applied
Physics Laboratory was supported by the Voyager Interstellar Mission
under NASA contract NNN06AA01C. The research at the Catholic University
of America was supported in part by NASA grant NNX12AC63G, and the
research at Goddard Spaceflight Center was supported by NASA contract
NNG14PN24P.
NR 39
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Z9 5
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2015
VL 809
IS 2
AR 121
DI 10.1088/0004-637X/809/2/121
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9EC
UT WOS:000361655100014
ER
PT J
AU Knizhnik, KJ
Antiochos, SK
DeVore, CR
AF Knizhnik, K. J.
Antiochos, S. K.
DeVore, C. R.
TI FILAMENT CHANNEL FORMATION VIA MAGNETIC HELICITY CONDENSATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: filaments, prominences; Sun: magnetic fields
ID GLOBAL SOLAR CORONA; DRIVEN VORTEX FLOWS; ACTIVE REGIONS; FIELDS; SUN;
PROMINENCES; CHIRALITY; DYNAMICS; RECONNECTION; SIMULATIONS
AB A major unexplained feature of the solar atmosphere is the accumulation of magnetic shear in the form of filament channels at photospheric polarity inversion lines (PILs). In addition to free energy, this shear represents magnetic helicity, which is conserved under reconnection. In this paper we address the problem of filament channel formation and show how filaments acquire their shear and magnetic helicity. The results of three-dimensional (3D) simulations using the Adaptively Refined Magnetohydrodynamics Solver are presented. Our findings support the model of filament channel formation by magnetic helicity condensation that was developed by Antiochos. We consider the small-scale photospheric twisting of a quasi-potential flux system that is bounded by a PIL and contains a coronal hole (CH). The magnetic helicity injected by the small-scale photospheric motions is shown to inverse cascade up to the largest allowable scales that define the closed flux system: the PIL and the CH. This process produces field lines that are both sheared and smooth, and are sheared in opposite senses at the PIL and the CH. The accumulated helicity and shear flux are shown to be in excellent quantitative agreement with the helicity condensation model. We present a detailed analysis of the simulations, including comparisons of our analytical and numerical results, and discuss their implications for observations.
C1 [Knizhnik, K. J.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21287 USA.
[Knizhnik, K. J.; Antiochos, S. K.; DeVore, C. R.] NASA Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Knizhnik, KJ (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21287 USA.
RI DeVore, C/A-6067-2015
OI DeVore, C/0000-0002-4668-591X
FU NASA's Heliophysics Theory and Supporting Research programs; NASA;
Catholic University of America; NASA Goddard Space Flight Center
FX We thank K. Dalmasse, S. Guidoni, A. Higginson, S. Masson, and K.
Muglach for illuminating discussions and helpful suggestions, and we
greatly appreciate J. Karpen's contribution of the artwork shown in
Figure 1. K.J.K. acknowledges support for this work by a cooperative
agreement between the Catholic University of America and the NASA
Goddard Space Flight Center, as well as additional funding received
through the NASA Earth and Space Science Fellowship program. The
participation of S.KA. and C.R.D. was sponsored by NASA's Heliophysics
Theory and Supporting Research programs. The numerical simulations were
supported by a grant of NASA High End Computing resources to C.R.D.
NR 66
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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 AUG 20
PY 2015
VL 809
IS 2
AR 137
DI 10.1088/0004-637X/809/2/137
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9EC
UT WOS:000361655100030
ER
PT J
AU Krivonos, RA
Tsygankov, SS
Lutovinov, AA
Tomsick, JA
Chakrabarty, D
Bachetti, M
Boggs, SE
Chernyakova, M
Christensen, FE
Craig, WW
Furst, F
Hailey, CJ
Harrison, FA
Lansbury, GB
Rahoui, F
Stern, D
Zhang, WW
AF Krivonos, Roman A.
Tsygankov, Sergey S.
Lutovinov, Alexander A.
Tomsick, John A.
Chakrabarty, Deepto
Bachetti, Matteo
Boggs, Steven E.
Chernyakova, Masha
Christensen, Finn E.
Craig, William W.
Fuerst, Felix
Hailey, Charles J.
Harrison, Fiona A.
Lansbury, George B.
Rahoui, Farid
Stern, Daniel
Zhang, William W.
TI NuSTAR DISCOVERY OF AN UNUSUALLY STEADY LONG-TERM SPIN-UP OF THE Be
BINARY 2RXP J130159.6-635806
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (2RXP J130159.6-635806); stars: emission-line, Be;
X-rays: binaries
ID X-RAY BINARIES; NEUTRON-STARS; PULSARS; PERIOD; ACCRETION; EVOLUTION;
EMISSION; CATALOG; ENERGY; LINE
AB We present spectral and timing analyses of Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the accreting X-ray pulsar 2RXP J130159.6-635806. The source was serendipitously observed during a campaign focused on the gamma-ray binary PSR B1259-63 and was later targeted for a dedicated observation. The spectrum has a typical shape for accreting X-ray pulsars, consisting of a simple power law with an exponential cutoff starting at similar to 7 keV with a folding energy of E-fold similar or equal to 18 keV. There is also an indication of the presence of a 6.4 keV iron line in the spectrum at the similar to 3 sigma significance level. NuSTAR measurements of the pulsation period reveal that the pulsar has undergone a strong and steady spin-up for the last 20 years. The pulsed fraction is estimated to be similar to 80%, and is constant with energy up to 40 keV. The power density spectrum shows a break toward higher frequencies relative to the current spin period. This, together with steady persistent luminosity, points to a long-term mass accretion rate high enough to bring the pulsar out of spin equilibrium.
C1 [Krivonos, Roman A.; Tomsick, John A.; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Krivonos, Roman A.; Tsygankov, Sergey S.; Lutovinov, Alexander A.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia.
[Tsygankov, Sergey S.] Univ Turku, Dept Phys & Astron, Tuorla Observ, FI-21500 Piikkio, Finland.
[Chakrabarty, Deepto] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Bachetti, Matteo] Univ Toulouse 3, Observ Midi Pyrenees, F-31400 Toulouse, France.
[Bachetti, Matteo] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse, France.
[Chernyakova, Masha] Dublin City Univ, Dublin 9, Ireland.
[Chernyakova, Masha] Dublin Inst Adv Studies, Dublin 2, Ireland.
[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.
[Fuerst, Felix; Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Lansbury, George B.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Rahoui, Farid] European So Observ, D-85748 Garching, Germany.
[Rahoui, Farid] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Krivonos, RA (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RI Boggs, Steven/E-4170-2015;
OI Krivonos, Roman/0000-0003-2737-5673; Boggs, Steven/0000-0001-9567-4224;
Bachetti, Matteo/0000-0002-4576-9337
FU NASA; ESA Member States; Russian Science Foundation [14-12-01287]
FX This research has made use of data obtained with NuSTAR, a project led
by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the
NUSTARDAS software package, jointly developed by the ASDC (Italy) and
Caltech (USA). This research has also made use of data obtained with
XMM-Newton, an ESA science mission with instruments and contributions
directly funded by ESA Member States. A.L. and S.T. acknowledge support
from Russian Science Foundation (grant 14-12-01287).
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 AUG 20
PY 2015
VL 809
IS 2
AR 140
DI 10.1088/0004-637X/809/2/140
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9EC
UT WOS:000361655100033
ER
PT J
AU Lansbury, GB
Gandhi, P
Alexander, DM
Assef, RJ
Aird, J
Annuar, A
Ballantyne, DR
Balokovic, M
Bauer, FE
Boggs, SE
Brandt, WN
Brightman, M
Christensen, FE
Civano, F
Comastri, A
Craig, WW
Del Moro, A
Grefenstette, BW
Hailey, CJ
Harrison, FA
Hickox, RC
Koss, M
LaMassa, SM
Luo, B
Puccetti, S
Stern, D
Treister, E
Vignali, C
Zappacosta, L
Zhang, WW
AF Lansbury, G. B.
Gandhi, P.
Alexander, D. M.
Assef, R. J.
Aird, J.
Annuar, A.
Ballantyne, D. R.
Balokovic, M.
Bauer, F. E.
Boggs, S. E.
Brandt, W. N.
Brightman, M.
Christensen, F. E.
Civano, F.
Comastri, A.
Craig, W. W.
Del Moro, A.
Grefenstette, B. W.
Hailey, C. J.
Harrison, F. A.
Hickox, R. C.
Koss, M.
LaMassa, S. M.
Luo, B.
Puccetti, S.
Stern, D.
Treister, E.
Vignali, C.
Zappacosta, L.
Zhang, W. W.
TI NuSTAR REVEALS EXTREME ABSORPTION IN z < 0.5 TYPE 2 QUASARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; HARD X-RAY; DIGITAL-SKY-SURVEY; SEYFERT 2
GALAXIES; COMPTON-THICK AGN; XMM-NEWTON OBSERVATIONS; ULTRALUMINOUS
INFRARED GALAXIES; RESOLUTION SPECTRAL TEMPLATES; LUMINOUS OBSCURED
QUASARS; APPROXIMATE-TO 2
AB The intrinsic column density (N-H) distribution of quasars is poorly known. At the high obscuration end of the quasar population and for redshifts z < 1, the X-ray spectra can only be reliably characterized using broad-band measurements that extend to energies above 10 keV. Using the hard X-ray observatory NuSTAR, along with archival Chandra and XMM-Newton data, we study the broad-band X-ray spectra of nine optically selected (from the SDSS), candidate Compton-thick (N-H > 1.5 x 10(24) cm(-2)) type 2 quasars (CTQSO2s); five new NuSTAR observations are reported herein, and four have been previously published. The candidate CTQSO2s lie at z < 0.5, have observed [O III] luminosities in the range 8.4< log(L-[O III]/L circle dot)< 9.6, and show evidence for extreme, Compton-thick absorption when indirect absorption diagnostics are considered. Among the nine candidate CTQSO2s, five are detected by NuSTAR in the high-energy (8-24 keV) band: two are weakly detected at the approximate to 3 sigma confidence level and three are strongly detected with sufficient counts for spectral modeling (greater than or similar to 90 net source counts at 8-24 keV). For these NuSTAR-detected sources direct (i.e., X-ray spectral) constraints on the intrinsic active galactic nucleus properties are feasible, and we measure column densities approximate to 2.5-1600 times higher and intrinsic (unabsorbed) X-ray luminosities approximate to 10-70 times higher than pre-NuSTAR constraints from Chandra and XMM-Newton. Assuming the NuSTAR-detected type 2 quasars are representative of other Compton-thick candidates, we make a correction to the N-H distribution for optically selected type 2 quasars as measured by Chandra and XMM-Newton for 39 objects. With this approach, we predict a Compton-thick fraction of f(CT) = 36(-12)(+14)%, although higher fractions (up to 76%) are possible if indirect absorption diagnostics are assumed to be reliable.
C1 [Lansbury, G. B.; Gandhi, P.; Alexander, D. M.; Annuar, A.; Del Moro, A.] Univ Durham, Ctr Extragalact Astron, Dept Phys, Durham DH1 3LE, England.
[Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17, Hants, England.
[Assef, R. J.] Univ Diego Portales, Nucleo Astron, Fac Ingn, Santiago, Chile.
[Aird, J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Balokovic, M.; Brightman, M.; Grefenstette, B. W.; Harrison, F. A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 22, Chile.
[Bauer, F. E.] Millennium Inst Astrophys, Santiago 7820436, 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.
[Civano, F.; LaMassa, S. M.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Civano, F.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Civano, F.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Koss, M.] Swiss Fed Inst Technol, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland.
[Puccetti, S.] ASDC ASI, I-00133 Rome, Italy.
[Puccetti, S.; Zappacosta, L.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Lansbury, GB (reprint author), Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England.
EM g.b.lansbury@durham.ac.uk
RI Comastri, Andrea/O-9543-2015; Vignali, Cristian/J-4974-2012; Brandt,
William/N-2844-2015; Boggs, Steven/E-4170-2015;
OI Comastri, Andrea/0000-0003-3451-9970; Lansbury,
George/0000-0002-5328-9827; Vignali, Cristian/0000-0002-8853-9611;
Puccetti, Simonetta/0000-0002-2734-7835; Brandt,
William/0000-0002-0167-2453; Boggs, Steven/0000-0001-9567-4224; Koss,
Michael/0000-0002-7998-9581; Ballantyne, David/0000-0001-8128-6976
FU Science and Technology Facilities Council (STFC) [ST/K501979/1,
ST/J003697/1, ST/I001573/1]; Leverhulme Trust; Gemini-CONICYT
[32120009]; ERC Advanced Grant FEEDBACK at the University of Cambridge;
NSF AST award [1008067]; NASA Earth and Space Science Fellowship Program
[NNX14AQ07H]; CONICYT-Chile [PFB-06/2007, FONDECYT 1141218, ACT1101];
Ministry of Economy, Development, and Tourism's Millennium Science
Initiative [IC120009]; Caltech NuSTAR subcontract [44A-1092750]; NASA
ADP grant [NNX10AC99G]; Caltech Kingsley visitor program; ASI/INAF
[I/037/12/0011/13]; NASA ADAP award [NNX12AE38G]; National Science
Foundation [1211096]; Swiss National Science Foundation
[PP00P2_138979/1]; NASA [NNG08FD60C]; National Aeronautics and Space
Administration
FX We thank the referee for a careful review, which has improved this work.
We acknowledge financial support from: the Science and Technology
Facilities Council (STFC) grants ST/K501979/1 (G.B.L.), ST/J003697/1
(P.G.), ST/I001573/1 (D.M.A. and A.D.M.); the Leverhulme Trust (D.M.A.);
Gemini-CONICYT grant 32120009 (R.J.A.); the ERC Advanced Grant FEEDBACK
at the University of Cambridge (J.A.); NSF AST award 1008067 (D.R.B.);
the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H
(M.B.); CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B.), FONDECYT
1141218 (F.E.B.), and "EMBIGGEN" Anillo ACT1101 (F.E.B.); the Ministry
of Economy, Development, and Tourism's Millennium Science Initiative
grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS
(F.E.B.); Caltech NuSTAR subcontract 44A-1092750 (W.N.B. and B.L.); NASA
ADP grant NNX10AC99G (W.N.B. and B.L.); the Caltech Kingsley visitor
program (A.C.); ASI/INAF grant I/037/12/0011/13 (A.C., S.P., C.V.); 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 Andrew Ptak and Jianjun Jia for the
useful correspondence. 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 112
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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 AUG 20
PY 2015
VL 809
IS 2
AR 115
DI 10.1088/0004-637X/809/2/115
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9EC
UT WOS:000361655100008
ER
PT J
AU Masiero, JR
Carruba, V
Mainzer, A
Bauer, JM
Nugent, C
AF Masiero, Joseph R.
Carruba, V.
Mainzer, A.
Bauer, J. M.
Nugent, C.
TI THE EUPHROSYNE FAMILY'S CONTRIBUTION TO THE LOW ALBEDO NEAR-EARTH
ASTEROIDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE minor planets; asteroids: general
ID SHORT-PERIOD COMETS; OBJECT POPULATION; SOLAR-SYSTEM; NEOWISE;
YARKOVSKY; TAXONOMY
AB The Euphrosyne asteroid family is uniquely situated at high inclination in the outer Main Belt, bisected by the n6 secular resonance. This large, low albedo family may thus be an important contributor to specific subpopulations of the near-Earth objects. We present simulations of the orbital evolution of Euphrosyne family members from the time of breakup to the present day, focusing on those members that move into near-Earth orbits. We find that family members typically evolve into a specific region of orbital element-space, with semimajor axes near similar to 3 AU, high inclinations, very large eccentricities, and Tisserand parameters similar to Jupiter family comets. Filtering all known Near-Earth objects (NEOs) with our derived orbital element limits, we find that the population of candidate objects is significantly lower in albedo than the overall NEO population, although many of our candidates are also darker than the Euphrosyne family, and may have properties more similar to comet nuclei. Followup characterization of these candidates will enable us to compare them to known family properties, and confirm which ones originated with the breakup of (31) Euphrosyne.
C1 [Masiero, Joseph R.; Mainzer, A.; Bauer, J. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Carruba, V.] Univ Estadual Paulista, Dept Matemat, BR-12516410 Guaratingueta, SP, Brazil.
[Nugent, C.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
RP Masiero, JR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-601, Pasadena, CA 91109 USA.
EM Joseph.Masiero@jpl.nasa.gov; vcarruba@feg.unesp.br;
amainzer@jpl.nasa.gov; bauer@scn.jpl.nasa.gov; cnugent@ipac.caltech.edu
RI Carruba, Valerio/H-5529-2012;
OI Carruba, Valerio/0000-0003-2786-0740; Masiero,
Joseph/0000-0003-2638-720X
FU NASA Planetary Geology and Geophysics grant; JPL internal Research and
Technology Development program; FAPESP [2014/06762-2]; National
Aeronautics and Space Administration; Planetary Science Division of the
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. J. M. was funded by a NASA
Planetary Geology and Geophysics grant, and through the JPL internal
Research and Technology Development program. V. C. was supported by the
FAPESP grant 2014/06762-2. The authors would like to thank UNESP, CAPES,
AAB, and FAPESP for supporting the 2014 Small Bodies Dynamics conference
in Ubatuba, Brazil, which inspired this work. The JPL High-Performance
Computing Facility used for our simulations is supported by the JPL
Office of the CIO. 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.
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 AUG 20
PY 2015
VL 809
IS 2
AR 179
DI 10.1088/0004-637X/809/2/179
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9EC
UT WOS:000361655100072
ER
PT J
AU Nichols, J
Huenemoerder, DP
Corcoran, MF
Waldron, W
Naze, Y
Pollock, AMT
Moffat, AFJ
Lauer, J
Shenar, T
Russell, CMP
Richardson, ND
Pablo, H
Evans, NR
Hamaguchi, K
Gull, T
Hamann, WR
Oskinova, L
Ignace, R
Hoffman, JL
Hole, KT
Lomax, JR
AF Nichols, J.
Huenemoerder, D. P.
Corcoran, M. F.
Waldron, W.
Naze, Y.
Pollock, A. M. T.
Moffat, A. F. J.
Lauer, J.
Shenar, T.
Russell, C. M. P.
Richardson, N. D.
Pablo, H.
Evans, N. R.
Hamaguchi, K.
Gull, T.
Hamann, W. -R.
Oskinova, L.
Ignace, R.
Hoffman, Jennifer L.
Hole, K. T.
Lomax, J. R.
TI A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE
ECLIPSING BINARY, delta ORIONIS Aa. II. X-RAY VARIABILITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; binaries: eclipsing; stars: individual ([HD 36486]delta
Ori A)
ID EARLY-TYPE STARS; SHORT-TERM VARIABILITY; HELIUM-LIKE IONS; O-TYPE
STARS; ABSORPTION COMPONENTS; LINE INTENSITIES; COLLIDING WINDS;
MAIN-SEQUENCE; ZETA-OPHIUCHI; TIME-SERIES
AB We present time-resolved and phase-resolved variability studies of an extensive X-ray high-resolution spectral data set of the delta Ori Aa binary system. The four observations, obtained with Chandra ACIS HETGS, have a total exposure time of approximate to 479 ks and provide nearly complete binary phase coverage. Variability of the total X-ray flux in the range of 5-25 is is confirmed, with a maximum amplitude of about +/- 15% within a single approximate to 125 ks observation. Periods of 4.76 and 2.04 days are found in the total X-ray flux, as well as an apparent overall increase in the flux level throughout the nine-day observational campaign. Using 40 ks contiguous spectra derived from the original observations, we investigate the variability of emission line parameters and ratios. Several emission lines are shown to be variable, including S XV, Si XIII, and Ne IX. For the first time, variations of the X-ray emission line widths as a function of the binary phase are found in a binary system, with the smallest widths at phi = 0.0 when the secondary delta Ori Aa2 is at the inferior conjunction. Using 3D hydrodynamic modeling of the interacting winds, we relate the emission line width variability to the presence of a wind cavity created by a wind-wind collision, which is effectively void of embedded wind shocks and is carved out of the X-ray-producing primary wind, thus producing phase-locked X-ray variability.
C1 [Nichols, J.; Lauer, J.; Evans, N. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Huenemoerder, D. P.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Corcoran, M. F.; Hamaguchi, K.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA.
[Corcoran, M. F.; Hamaguchi, K.] NASA GSFC, XRay Astrophys Lab, Greenbelt, MD 20771 USA.
[Waldron, W.] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Naze, Y.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Pollock, A. M. T.] Univ Liege, FNRS Dept AGO, B-4000 Liege, Belgium.
[Moffat, A. F. J.; Richardson, N. D.; Pablo, H.] European Space Agcy, XMM Newton Sci Operat Ctr, European Space Astron Ctr, E-28691 Villanueva De La Canada, Spain.
[Shenar, T.; Hamann, W. -R.; Oskinova, L.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Hamaguchi, K.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Gull, T.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Ignace, R.] NASA GSFC, Greenbelt, MD 20771 USA.
[Hoffman, Jennifer L.] E Tennessee State Univ, Phys & Astron, Johnson City, TN 37614 USA.
[Hole, K. T.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Lomax, J. R.] Weber State Univ, Dept Phys, Ogden, UT 84408 USA.
[Russell, C. M. P.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Russell, C. M. P.] NASA Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
RP Nichols, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU National Aeronautics and Space Administration through Chandra Award
[GO3-14015A, G03-14015E, GO3-14015G]; National Aeronautics Space
Administration [NAS8-03060]; NASA through the Smithsonian Astrophysical
Observatory [SV3-73016]; Fonds National de la Recherche Scientifique
(Belgium); Communaute Francaise de Belgique; PRODEX XMM and Integral
contracts; Action de Recherche Concertee (CFWB-Academie Wallonie
Europe); NSRC (Canada); FRQNT (Quebec); CRAQ (Centre de Recherche en
Astrophysique du Quebec) fellowship; DLR [50 OR 1302]; Chandra X-ray
Center NASA [NAS8-03060]; NASA [NNX13AF40G]; NSF [AST-0807477]
FX The authors acknowledge the constructive comments of the anomymous
referee. M.F.C., J.S.N., W.L.W., C.M.P.R., and K.H. are grateful for
support provided by the National Aeronautics and Space Administration
through Chandra Award Number GO3-14015A, G03-14015E, and GO3-14015G
issued by the Chandra X-ray Observatory Center, which is operated by the
Smithsonian Astrophysical Observatory for and on behalf of the National
Aeronautics Space Administration under contract NAS8-03060. D.P.H. was
supported by NASA through the Smithsonian Astrophysical Observatory
contract SV3-73016 to MIT for the Chandra X-ray Center and Science
Instruments. Y.N. acknowledges support from the Fonds National de la
Recherche Scientifique (Belgium), the Communaute Francaise de Belgique,
the PRODEX XMM and Integral contracts, and the Action de Recherche
Concertee (CFWB-Academie Wallonie Europe). A.F.J.M. is grateful for
financial aid from NSRC (Canada) and FRQNT (Quebec). N.D.R. gratefully
acknowledges his CRAQ (Centre de Recherche en Astrophysique du Quebec)
fellowship. L.M.O. acknowledges support from DLR grant 50 OR 1302.
N.R.E. is grateful for support from the Chandra X-ray Center NASA
Contract NAS8-03060. J.L.H. acknowledges support from NASA award
NNX13AF40G and NSF award AST-0807477. M.F.C., J.S.N., and K.H. also
acknowledge helpful discussions with John Houck and Michael Nowak on
data analysis with ISIS, and Craig Anderson for technical support. This
research has made use of data and/or software provided by the High
Energy Astrophysics Science Archive Research Center (HEASARC), which is
a service of the Astrophysics Science Division at NASA/GSFC and the High
Energy Astrophysics Division of the Smithsonian Astrophysical
Observatory. This research made use of the Chandra Transmission Grating
Catalog and archive (http://tgcat.mit.edu). This research also has made
use of NASA's Astrophysics Data System.
NR 80
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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 AUG 20
PY 2015
VL 809
IS 2
AR 133
DI 10.1088/0004-637X/809/2/133
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9EC
UT WOS:000361655100026
ER
PT J
AU Pablo, H
Richardson, ND
Moffat, AFJ
Corcoran, M
Shenar, T
Benvenuto, O
Fuller, J
Naze, Y
Hoffman, JL
Miroshnichenko, A
Apellaniz, JM
Evans, N
Eversberg, T
Gayley, K
Gull, T
Hamaguchi, K
Hamann, WR
Henrichs, H
Hole, T
Ignace, R
Iping, R
Lauer, J
Leutenegger, M
Lomax, J
Nichols, J
Oskinova, L
Owocki, S
Pollock, A
Russell, CMP
Waldron, W
Buil, C
Garrel, T
Graham, K
Heathcote, B
Lemoult, T
Li, D
Mauclaire, B
Potter, M
Ribeiro, J
Matthews, J
Cameron, C
Guenther, D
Kuschnig, R
Rowe, J
Rucinski, S
Sasselov, D
Weiss, W
AF Pablo, Herbert
Richardson, Noel D.
Moffat, Anthony F. J.
Corcoran, Michael
Shenar, Tomer
Benvenuto, Omar
Fuller, Jim
Naze, Yael
Hoffman, Jennifer L.
Miroshnichenko, Anatoly
Apellaniz, Jesus Maiz
Evans, Nancy
Eversberg, Thomas
Gayley, Ken
Gull, Ted
Hamaguchi, Kenji
Hamann, Wolf-Rainer
Henrichs, Huib
Hole, Tabetha
Ignace, Richard
Iping, Rosina
Lauer, Jennifer
Leutenegger, Maurice
Lomax, Jamie
Nichols, Joy
Oskinova, Lida
Owocki, Stan
Pollock, Andy
Russell, Christopher M. P.
Waldron, Wayne
Buil, Christian
Garrel, Thierry
Graham, Keith
Heathcote, Bernard
Lemoult, Thierry
Li, Dong
Mauclaire, Benjamin
Potter, Mike
Ribeiro, Jose
Matthews, Jaymie
Cameron, Chris
Guenther, David
Kuschnig, Rainer
Rowe, Jason
Rucinski, Slavek
Sasselov, Dimitar
Weiss, Werner
TI A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE
ECLIPSING BINARY, delta ORIONIS Aa. III. ANALYSIS OF OPTICAL PHOTOMETRIC
(MOST) AND SPECTROSCOPIC (GROUND BASED) VARIATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; binaries: eclipsing; stars: early-type; stars:
individual (delta Ori A); stars: mass-loss; stars: variables: general
ID APSIDAL MOTION; STARS; SYSTEM; PULSATIONS; KOI-54; SPECTRA; ORBITS;
SPOTS; ORI
AB We report on both high-precision photometry from the Microvariability and Oscillations of Stars (MOST) space telescope and ground-based spectroscopy of the triple system delta Ori A, consisting of a binary O9.5II+early-B (Aa1 and Aa2) with P = 5.7 days, and a more distant tertiary (O9 IV P > 400 years). This data was collected in concert with X-ray spectroscopy from the Chandra X-ray Observatory. Thanks to continuous coverage for three weeks, the MOST light curve reveals clear eclipses between Aa1 and Aa2 for the first time in non-phased data. From the spectroscopy, we have a well-constrained radial velocity (RV) curve of Aa1. While we are unable to recover RV variations of the secondary star, we are able to constrain several fundamental parameters of this system and determine an approximate mass of the primary using apsidal motion. We also detected second order modulations at 12 separate frequencies with spacings indicative of tidally influenced oscillations. These spacings have never been seen in a massive binary, making this system one of only a handful of such binaries that show evidence for tidally induced pulsations.
C1 [Pablo, Herbert; Richardson, Noel D.; Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Pablo, Herbert; Richardson, Noel D.; Moffat, Anthony F. J.] Univ Montreal, CRAQ, Montreal, PQ H3C 3J7, Canada.
[Corcoran, Michael; Hamaguchi, Kenji] NASA GSFC, CRESST, Greenbelt, MD 20771 USA.
[Corcoran, Michael; Hamaguchi, Kenji] NASA GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Corcoran, Michael; Iping, Rosina] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Shenar, Tomer; Hamann, Wolf-Rainer; Oskinova, Lida] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Benvenuto, Omar] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, RA-1900 Buenos Aires, DF, Argentina.
[Benvenuto, Omar] UNLP, CONICET, CCT, IALP, La Plata, Buenos Aires, Argentina.
[Fuller, Jim] CALTECH, Walter Burke Inst Theoret Phys, TAPIR, Pasadena, CA 91125 USA.
[Fuller, Jim; Leutenegger, Maurice] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Naze, Yael] Univ Liege, FNRS Dept AGO, B-4000 Liege, Belgium.
[Hoffman, Jennifer L.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Miroshnichenko, Anatoly] Univ N Carolina, Dept Phys & Astron, Greensboro, NC 27402 USA.
[Apellaniz, Jesus Maiz] Ctr Astrobiol CSIC INTA, E-28691 Villanueva De La Caada, Spain.
[Evans, Nancy; Lauer, Jennifer; Nichols, Joy] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Eversberg, Thomas] Schnorringen Telescope Sci Inst, Waldbrol, Germany.
[Gayley, Ken] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Gull, Ted] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Henrichs, Huib] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Hole, Tabetha; Ignace, Richard] E Tennessee State Univ, Dept Phys & Astron, Johnson City, TN 37614 USA.
[Lomax, Jamie] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Owocki, Stan] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Pollock, Andy] European Space Agcy, E-28691 Madrid, Spain.
[Russell, Christopher M. P.] NASA Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Russell, Christopher M. P.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Waldron, Wayne] Eureka Sci Inc, Oakland, CA 94602 USA.
[Buil, Christian] Castanet Tolosan Observ, F-31320 Castanet Tolosan, France.
[Garrel, Thierry] Observ Juvignac, F-34990 Juvignac, France.
[Heathcote, Bernard] Barfold Observ, Glenhope, Vic 3444, Australia.
[Lemoult, Thierry] Chelles Observ, F-77500 Chelles, France.
[Li, Dong] Jade Observ, Tianjin 300251, Peoples R China.
[Mauclaire, Benjamin] Observ Val Arc, F-13530 Trets, France.
[Ribeiro, Jose] Observ Inst Geog Exercito, Lisbon, Portugal.
[Matthews, Jaymie; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Cameron, Chris] Cape Breton Univ, Dept Math Phys & Geol, Sydney, NS B1P 6L2, Canada.
[Guenther, David] St Marys Univ, Inst Computat Astrophys, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Kuschnig, Rainer] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Rowe, Jason] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rucinski, Slavek] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Pablo, H (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada.
EM hpablo@astro.umontreal.ca; richardson@astro.umontreal.ca
FU Chandra grant [GO3-14015A, GO3-14015E]; Fonds National de la Recherche
Scientifique (Belgium); Communaute Francaise de Belgique; PRODEX
XMMAction de Recherche Concertee (CFWB-Academie Wallonie Europe); CRAQ
(Centre de Recherche en Astrophysique du Quebec); Spanish Government
Ministerio de Economia y Competitividad (MINECO) [AYA2010-15 081,
AYA2010-17 631, AYA2013-40 611-P]; Consejeria de Educacion of the Junta
de Andalucia [P08-TIC-4075]; Austrian Science Fund (FWF); Chandra X-ray
Center NASA [NAS8-03060]; NASA [NNX13AF40G]; NSF [AST-0807477]
FX M.F.C., J.S.N., W.L.W., and K.H. are grateful for support via Chandra
grant GO3-14015A and GO3-14015E. Y.N. acknowledges support from the
Fonds National de la Recherche Scientifique (Belgium), the Communaute
Francaise de Belgique, the PRODEX XMM and Integral contracts, and the
Action de Recherche Concertee (CFWB-Academie Wallonie Europe). N.D.R.
gratefully acknowledges his CRAQ (Centre de Recherche en Astrophysique
du Quebec) fellowship. A.F.J.M., D.B.G., J.M.M., and S.M.R. are grateful
for financial aid to NSERC (Canada). A.F.J.M. and H.P. also thank FRQNT
(Quebec) and the Canadian Space Agency. J.M.A. acknowledges support from
(a) the Spanish Government Ministerio de Economia y Competitividad
(MINECO) through grants AYA2010-15 081, AYA2010-17 631, and AYA2013-40
611-P and (b) the Consejeria de Educacion of the Junta de Andalucia
through grant P08-TIC-4075. R.K. and W.W. acknowledge support by the
Austrian Science Fund (FWF). N.R.E. is grateful for support from the
Chandra X-ray Center NASA Contract NAS8-03060. J.L.H. acknowledges
support from NASA award NNX13AF40G and NSF award AST-0807477.
NR 61
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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 AUG 20
PY 2015
VL 809
IS 2
AR 134
DI 10.1088/0004-637X/809/2/134
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9EC
UT WOS:000361655100027
ER
PT J
AU Shenar, T
Oskinova, L
Hamann, WR
Corcoran, MF
Moffat, AFJ
Pablo, H
Richardson, ND
Waldron, WL
Huenemoerder, DP
Apellaniz, JM
Nichols, JS
Todt, H
Naze, Y
Hoffman, JL
Pollock, AMT
Negueruela, I
AF Shenar, T.
Oskinova, L.
Hamann, W. -R.
Corcoran, M. F.
Moffat, A. F. J.
Pablo, H.
Richardson, N. D.
Waldron, W. L.
Huenemoerder, D. P.
Maiz Apellaniz, J.
Nichols, J. S.
Todt, H.
Naze, Y.
Hoffman, J. L.
Pollock, A. M. T.
Negueruela, I.
TI A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE
ECLIPSING BINARY, delta ORIONIS Aa. IV. A MULTIWAVELENGTH, NON-LTE
SPECTROSCOPIC ANALYSIS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; binaries: eclipsing; stars: early-type; stars:
individual ([HD 36486]delta Ori A); X-rays: stars
ID O-TYPE STARS; RADIATION-DRIVEN WINDS; BLANKETED MODEL ATMOSPHERES;
EMISSION-LINE-PROFILES; B-TYPE SUPERGIANTS; HELIUM-LIKE IONS; STELLAR
WINDS; GALACTIC O; LOSS RATES; COMPOSITE SPECTRA
AB Eclipsing systems of massive stars allow one to explore the properties of their components in great detail. We perform a multi-wavelength, non-LTE analysis of the three components of the massive multiple system delta Ori A, focusing on the fundamental stellar properties, stellar winds, and X-ray characteristics of the system. The primary's distance-independent parameters turn out to be characteristic for its spectral type (O9.5 II), but usage of the Hipparcos parallax yields surprisingly low values for the mass, radius, and luminosity. Consistent values follow only if delta Ori lies at about twice the Hipparcos distance, in the vicinity of the sigma-Orionis cluster. The primary and tertiary dominate the spectrum and leave the secondary only marginally detectable. We estimate the V-band magnitude difference between primary and secondary to be Delta V approximate to 2.(m)8. The inferred parameters suggest that the secondary is an early B-type dwarf (approximate to B1 V), while the tertiary is an early B-type subgiant (approximate to B0 IV). We find evidence for rapid turbulent velocities (similar to 200 km s(-1)) and wind inhomogeneities, partially optically thick, in the primary's wind. The bulk of the X-ray emission likely emerges from the primary's stellar wind (logL(X)/L-Bol approximate to -6.85), initiating close to the stellar surface at R-0 similar to 1.1 R-*. Accounting for clumping, the mass-loss rate of the primary is found to be log (M) over dot approximate to -6.4 (M-circle dot yr(-1))., which agrees with hydrodynamic predictions, and provides a consistent picture along the X-ray, UV, optical, and radio spectral domains.
C1 [Shenar, T.; Oskinova, L.; Hamann, W. -R.; Todt, H.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Corcoran, M. F.] NASA Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Corcoran, M. F.] NASA Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Moffat, A. F. J.; Pablo, H.; Richardson, N. D.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Moffat, A. F. J.; Pablo, H.; Richardson, N. D.] Univ Montreal, CRAQ, Montreal, PQ H3C 3J7, Canada.
[Waldron, W. L.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Huenemoerder, D. P.] MIT, Kalvi Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Maiz Apellaniz, J.] INTA CSIC, Ctr Astrobiol, E-28691 Madrid, Spain.
[Nichols, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Naze, Y.] Univ Liege, Inst Astrophys & Geophys, Grp Astrophys Hautes Energies, B-4000 Sart Tilman Par Liege, Belgium.
[Hoffman, J. L.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Pollock, A. M. T.] European Space Agcy, XMM Newton Sci Operat Ctr, European Space Astron Ctr, E-28691 Villanueva De La Canada, Spain.
[Negueruela, I.] Univ Alicante, Escuela Politecn Super, Dept Fis Ingn Sistemas & Teoria Senal, E-03080 Alicante, Spain.
RP Shenar, T (reprint author), Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany.
FU Leibniz Graduate School for Quantitative Spectroscopy in Astrophysics;
Leibniz Institute for Astrophysics Potsdam (AIP); institute of Physics
and Astronomy of the University of Potsdam; DLR [50 OR 1302]; Chandra
grants [GO3-14015A, GO3-14015E]; NSERC (Canada); FRQNT (Quebec); Spanish
Government Ministerio de Economia y Competitividad (MINECO) [AYA2010-15
081, AYA2010-17 631]; Consejeria de Educacion of the Junta de Andaluc ia
[P08-TIC-4075]; Centre du Recherche en Astrophysique du Quebec (CRAQ)
fellowship; Fonds National de la Recherche Scientifique (Belgium);
Communaute Francaise de Belgique; PRODEX XMM and Integral contracts;
"Action de Recherche Concertee" (CFWB-Academie Wallonie Europe); NASA
[NNX13AF40G]; NSF [AST-0807477]; Spanish Mineco
[AYA2012-39364-C02-01/02]; European Union
FX We thank the anonymous referee for constructive comments which helped to
improve our paper. T.S. is grateful for financial support from the
Leibniz Graduate School for Quantitative Spectroscopy in Astrophysics, a
joint project of the Leibniz Institute for Astrophysics Potsdam (AIP)
and the institute of Physics and Astronomy of the University of Potsdam.
L.M.O. acknowledges support from DLR grant 50 OR 1302. We thank A.
Valeev and S. Fabrika for kindly providing us with an optical spectrum
of the system. We thank T. J. Henry and J. A. Caballero for fruitful
discussions regarding system's distance. M.F.C., J.S.N., and W.L.W. are
grateful for support via Chandra grants GO3-14015A and GO3-14015E.
A.F.J.M. acknowledges financial aid from NSERC (Canada) and FRQNT
(Quebec). J.M.A. acknowledges support from (a) the Spanish Government
Ministerio de Economia y Competitividad (MINECO) through grants
AYA2010-15 081 and AYA2010-17 631 and (b) the Consejeria de Educacion of
the Junta de Andaluc ia through grant P08-TIC-4075. Caballero N.D.R.
gratefully acknowledges his Centre du Recherche en Astrophysique du
Quebec (CRAQ) fellowship. Y.N. acknowledges support from the Fonds
National de la Recherche Scientifique (Belgium), the Communaute
Francaise de Belgique, the PRODEX XMM and Integral contracts, and the
"Action de Recherche Concertee" (CFWB-Academie Wallonie Europe). J.L.H.
acknowledges support from NASA award NNX13AF40G and NSF award
AST-0807477. I.N. is supported by the Spanish Mineco under grant
AYA2012-39364-C02-01/02, and the European Union.
NR 146
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2015
VL 809
IS 2
AR 135
DI 10.1088/0004-637X/809/2/135
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9EC
UT WOS:000361655100028
ER
PT J
AU Woodward, CE
Kelley, MSP
Harker, DE
Ryan, EL
Wooden, DH
Sitko, ML
Russell, RW
Reach, WT
de Pater, I
Kolokolova, L
Gehrz, RD
AF Woodward, Charles E.
Kelley, Michael S. P.
Harker, David E.
Ryan, Erin L.
Wooden, Diane H.
Sitko, Michael L.
Russell, Ray W.
Reach, William T.
de Pater, Imke
Kolokolova, Ludmilla
Gehrz, Robert D.
TI SOFIA INFRARED SPECTROPHOTOMETRY OF COMET C/2012 K1 (PAN-STARRS)
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; comets: individual (C/2012 K1 Pan-STARRS); dust,
extinction
ID O1 HALE-BOPP; INTERPLANETARY DUST PARTICLES; DIFFUSE
INTERSTELLAR-MEDIUM; NARROW-BAND PHOTOMETRY; JUPITER-FAMILY COMETS; DEEP
IMPACT; C/1995 O1; CRYSTALLINE SILICATES; SOLAR NEBULA; PROTOPLANETARY
DISKS
AB We present pre-perihelion infrared 8-31 mu m spectrophotometric and imaging observations of comet C/2012 K1 (Pan-STARRS), a dynamically new Oort Cloud comet, conducted with NASA's Stratospheric Observatory for Infrared Astronomy facility (+FORCAST) in 2014 June. As a "new" comet (first inner solar system passage), the coma grain population may be extremely pristine, unencumbered by a rime and insufficiently irradiated by the Sun to carbonize its surface organics. The comet exhibited a weak 10 mu m silicate feature similar or equal to 1.18 +/- 0.03 above the underlying best-fit 215.32 +/- 0.95 K continuum blackbody. Thermal modeling of the observed spectral energy distribution indicates that the coma grains are fractally solid with a porosity factor D = 3 and the peak in the grain size distribution, a(peak) = 0.6 mu m, large. The sub-micron coma grains are dominated by amorphous carbon, with a silicate-to-carbon ratio of 0.80(-0.20)(+0.25).The silicate crystalline mass fraction is 0.20(-0.10)(+0.30), similar to with other dynamically new comets exhibiting weak 10 mu m silicate features. The bolometric dust albedo of the coma dust is 0.14 +/- 0.01 at a phase angle of 34 degrees.76, and the average dust production rate, corrected to zero phase, at the epoch of our observations was Af rho similar or equal to 5340 cm.
C1 [Woodward, Charles E.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Kelley, Michael S. P.; Ryan, Erin L.; Kolokolova, Ludmilla] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Harker, David E.] Univ Calif San Diego, Dept 0424, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Wooden, Diane H.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Sitko, Michael L.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
[Russell, Ray W.] Aerosp Corp, Los Angeles, CA 90009 USA.
[Reach, William T.] NASA, Ames Res Ctr, USRA SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[de Pater, Imke] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Gehrz, Robert D.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
RP Woodward, CE (reprint author), Univ Minnesota, Minnesota Inst Astrophys, 116 Church St SE, Minneapolis, MN 55455 USA.
EM chickw024@gmail.com
OI Reach, William/0000-0001-8362-4094
FU Universities Space Research Association (USRA)/NASA [NAS2-97001]; NASA
Planetary Astronomy Program [12-PAST12-0016, NNX13AJ11G]; Aerospace
Corporation by the Independent Research and Development program
FX C.E.W. and his team acknowledge support from Universities Space Research
Association (USRA)/NASA contract NAS2-97001. C.E.W., M.S.K., and D.E.H.
also acknowledge support from NASA Planetary Astronomy Program grant
12-PAST12-0016, while C.E.W. and E.L.R. also note support from NASA
Planetary Astronomy Program grant NNX13AJ11G. The authors would also
like to acknowledge the support and insight of Drs. J. DeBuzier and L.
A. Helton of the SOFIA Science Ctr. for their assistance with flight
planning and data reduction activities. This work is supported at The
Aerospace Corporation by the Independent Research and Development
program. We also thank the comments and suggestions of an anonymous
referee that improved the clarity of our work.
NR 111
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2015
VL 809
IS 2
AR 181
DI 10.1088/0004-637X/809/2/181
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9EC
UT WOS:000361655100074
ER
PT J
AU Young, AH
Mroczkowski, T
Romero, C
Sayers, J
Balestra, I
Clarke, TE
Czakon, N
Devlin, M
Dicker, SR
Ferrari, C
Girardi, M
Golwala, S
Intema, H
Korngut, PM
Mason, BS
Mercurio, A
Nonino, M
Reese, ED
Rosati, P
Sarazin, C
Umetsu, K
AF Young, Alexander H.
Mroczkowski, Tony
Romero, Charles
Sayers, Jack
Balestra, Italo
Clarke, Tracy E.
Czakon, Nicole
Devlin, Mark
Dicker, Simon R.
Ferrari, Chiara
Girardi, Marisa
Golwala, Sunil
Intema, Huib
Korngut, Phillip M.
Mason, Brian S.
Mercurio, Amata
Nonino, Mario
Reese, Erik D.
Rosati, Piero
Sarazin, Craig
Umetsu, Keiichi
TI MEASUREMENTS OF THE SUNYAEV-ZEL'DOVICH EFFECT IN MACS J0647.7+7015 AND
MACS J1206.2-0847 AT HIGH ANGULAR RESOLUTION WITH MUSTANG
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; galaxies:
clusters: individual (MACS J0647.7+7015, MACS J1206.2-0847); galaxies:
clusters: intracluster medium; X-rays: galaxies: clusters
ID MASSIVE GALAXY CLUSTERS; GREEN-BANK-TELESCOPE; GREATER-THAN 0.5;
PRESSURE PROFILES; SCALING RELATIONS; LENSING ANALYSIS; RELATIVISTIC
CORRECTIONS; INTRACLUSTER MEDIUM; COMPLETE SAMPLE; RX J1347-1145
AB We present high resolution (9 '') imaging of the Sunyaev-Zel'dovich Effect (SZE) toward two massive galaxy clusters, MACS J0647.7+ 7015 (z = 0.591) and MACS J1206.2-0847 (z = 0.439). We compare these 90 GHz measurements, taken with the Multiplexed Squid/TES Array at Ninety Gigahertz (MUSTANG) receiver on the Green Bank Telescope, with generalized Navarro-Frenk-White (gNFW) models derived from Bolocam 140 GHz SZE data as well as maps of the thermal gas derived from Chandra X-ray observations. We adopt a serial-fitting approach, in which gNFW models are first fit to the Bolocam data and then compared to the MUSTANG data to determine an overall best-fit model. For MACS J0647.7+ 7015, we find a gNFW profile with core slope parameter gamma = 0.9 fits the MUSTANG image with chi(2)(red) = 1.005 and probability to exceed (PTE) = 0.34. For MACS J1206.2-0847, we find gamma = 0.7, chi(2)(red) = 0.993 and PTE = 0.70. In addition, we find a significant (> 3 sigma) residual SZE feature in MACS J1206.2-0847 coincident with a group of galaxies identified in Very Large Telescope data and filamentary structure found in a weak-lensing mass reconstruction. We suggest the detected sub-structure may be the SZE decrement from a low mass foreground group or an infalling group. Giant Metrewave Radio Telescope measurements at 610 MHz reveal diffuse extended radio emission to the west, which we posit is either an active galactic nucleus-driven radio lobe, a bubble expanding away from disturbed gas associated with the SZE signal, or a bubble detached and perhaps re-accelerated by sloshing within the cluster. Using the spectroscopic redshifts available,we find evidence for a foreground (z = 0.423) or infalling group, coincident with the residual SZE feature.
C1 [Young, Alexander H.; Devlin, Mark; Dicker, Simon R.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Young, Alexander H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mroczkowski, Tony; Clarke, Tracy E.] US Naval Res Lab, Washington, DC 20375 USA.
[Romero, Charles; Mason, Brian S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Romero, Charles; Sarazin, Craig] Univ Virginia, Dept Astron, Charlottesville, VA 22901 USA.
[Sayers, Jack; Golwala, Sunil; Korngut, Phillip M.] CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA.
[Balestra, Italo; Girardi, Marisa; Nonino, Mario] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy.
[Czakon, Nicole; Umetsu, Keiichi] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Ferrari, Chiara] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR 7293, F-06300 Nice, France.
[Girardi, Marisa] Univ Trieste, Dipartimento Fis, Sez Astron, I-34143 Trieste, Italy.
[Intema, Huib] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Mercurio, Amata] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Reese, Erik D.] Moorpark Coll, Dept Phys Astron & Engn, Moorpark, CA 93021 USA.
[Rosati, Piero] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy.
RP Young, AH (reprint author), Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA.
EM alyoung@sas.upenn.edu
RI Intema, Huib/D-1438-2012;
OI Intema, Huib/0000-0002-5880-2730; Nonino, Mario/0000-0001-6342-9662;
Balestra, Italo/0000-0001-9660-894X; Mroczkowski,
Tony/0000-0003-3816-5372; Umetsu, Keiichi/0000-0002-7196-4822
FU Gordon and Betty Moore Foundation; Jet Propulsion Laboratory Research
and Technology Development Program; National Science Council of Taiwan
[NSC100-2112-M-001-008-MY3]; ESO VLT Large Programme [186.A-0798]; 6.1
Base funding; NSF [AST-0607654]; NASA [PF0-110077]; NASA through a
National Research Council Research Associateship Award at the U.S. Naval
Research Laboratory; NRAO Student Observing Support (SOS); NASA; Norris
Foundation CCAT Postdoctoral Program Fellowship; [NSF/AST-1309032];
[NSF/AST-9618798]; [NSF/AST-0098737]; [NSF/AST-9980846];
[NSF/AST-0229008]; [NSF/AST-0206158]; [NSF/AST-1313447]
FX We thank the anonymous referee for the useful comments that helped
improve this manuscript. The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. The GBT+MUSTANG observations
presented here were obtained with telescope time allocated under NRAO
proposal IDs AGBT11A009, and AGBT11B001. Additional funding was provided
by NSF/AST-1309032. The Bolocam observations presented here were
obtained operating from the Caltech Submillimeter Observatory, which,
when the data used in this analysis were taken, was operated by the
California Institute of Technology under cooperative agreement with the
National Science Foundation. Bolocam was constructed and commissioned
using funds from NSF/AST-9618798, NSF/AST-0098737, NSF/AST-9980846,
NSF/AST-0229008, and NSF/AST-0206158. Bolocam observations were
partially supported by the Gordon and Betty Moore Foundation, the Jet
Propulsion Laboratory Research and Technology Development Program, as
well as the National Science Council of Taiwan grant
NSC100-2112-M-001-008-MY3. The MACS J1206.2-0847 spectroscopic data were
based on the ESO VLT Large Programme (prog. ID 186.A-0798, PI: P.
Rosati). Basic research in radio astronomy at the Naval Research
Laboratory is supported by 6.1 Base funding. The late night assistance
of the GBT operators Greg Monk, Donna Stricklin, Barry Sharp and Dave
Rose was much appreciated during the observations. Much of the work
presented here was supported by NSF grant AST-0607654. Support for TM
was provided by NASA through the Einstein Fellowship Program, grant
PF0-110077, and through a National Research Council Research
Associateship Award at the U.S. Naval Research Laboratory. Support for
P.K. and A.Y. was provided by the NRAO Student Observing Support (SOS)
and NASA Post-doctoral Fellowship programs. J.S. was partially supported
by a Norris Foundation CCAT Postdoctoral Program Fellowship and by
NSF/AST-1313447.
NR 58
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U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2015
VL 809
IS 2
AR 185
DI 10.1088/0004-637X/809/2/185
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9EC
UT WOS:000361655100078
ER
PT J
AU Viero, MP
Moncelsi, L
Quadri, RF
Bethermin, M
Bock, J
Burgarella, D
Chapman, SC
Clements, DL
Conley, A
Conversi, L
Duivenvoorden, S
Dunlop, JS
Farrah, D
Franceschini, A
Halpern, M
Ivison, RJ
Lagache, G
Magdis, G
Marchetti, L
Alvarez-Marquez, J
Marsden, G
Oliver, SJ
Page, MJ
Perez-Fournon, I
Schulz, B
Scott, D
Valtchanov, I
Vieira, JD
Wang, L
Wardlow, J
Zemcov, M
AF Viero, M. P.
Moncelsi, L.
Quadri, R. F.
Bethermin, M.
Bock, J.
Burgarella, D.
Chapman, S. C.
Clements, D. L.
Conley, A.
Conversi, L.
Duivenvoorden, S.
Dunlop, J. S.
Farrah, D.
Franceschini, A.
Halpern, M.
Ivison, R. J.
Lagache, G.
Magdis, G.
Marchetti, L.
Alvarez-Marquez, J.
Marsden, G.
Oliver, S. J.
Page, M. J.
Perez-Fournon, I.
Schulz, B.
Scott, Douglas
Valtchanov, I.
Vieira, J. D.
Wang, L.
Wardlow, J.
Zemcov, M.
TI HERMES: CURRENT COSMIC INFRARED BACKGROUND ESTIMATES CAN BE EXPLAINED BY
KNOWN GALAXIES AND THEIR FAINT COMPANIONS AT z < 4
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmology: observations; galaxies: evolution; infrared: galaxies;
large-scale structure of universe; submillimeter: galaxies
ID OBSCURED STAR-FORMATION; STELLAR MASS FUNCTIONS; DEEP-FIELD-SOUTH;
QUIESCENT GALAXIES; SUBMILLIMETER GALAXIES; LUMINOSITY FUNCTIONS; NUMBER
COUNTS; REDSHIFT; DUSTY; IMAGES
AB We report contributions to cosmic infrared background (CIB) intensities originating from known galaxies and their faint companions at submillimeter wavelengths. Using the publicly available UltraVISTA catalog and maps at 250, 350, and 500 mu m from the Herschel Multi-tiered Extragalactic Survey, we perform a novel measurement that exploits the fact that uncataloged sources may bias stacked flux densities-particularly if the resolution of the image is poor-and intentionally smooth the images before stacking and summing intensities. By smoothing the maps we are capturing the contribution of faint (undetected in K-S similar to 23.4) sources that are physically associated, or correlated, with the detected sources. We find that the cumulative CIB increases with increased smoothing, reaching 9.82 +/- 0.78, 5.77 +/- 0.43 and 2.32 +/- 0.19 nWm(-2) sr(-1) at 250, 350, and 500 mu m at 300 arcsec FWHM. This corresponds to a fraction of the fiducial CIB of 0.94 +/- 0.23, 1.07 +/- 0.31, and 0.97 +/- 0.26 at 250, 350, and 500 mu m, where the uncertainties are dominated by those of the absolute CIB. We then propose, with a simple model combining parametric descriptions for stacked flux densities and stellar mass functions, that emission from galaxies with log(M/M-circle dot) > 8.5 can account for most of the measured total intensities and argue against contributions from extended, diffuse emission. Finally, we discuss prospects for future survey instruments to improve the estimates of the absolute CIB levels, and observe any potentially remaining emission at z > 4.
C1 [Viero, M. P.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Viero, M. P.; Moncelsi, L.; Bock, J.; Schulz, B.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA.
[Quadri, R. F.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Bethermin, M.] Univ Paris Diderot, Lab AIM Paris Saclay, CE Saclay, CEA,DSM,Irfu,CNRS, F-91191 Gif Sur Yvette, France.
[Bethermin, M.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Bethermin, M.] CNRS, UMR 8617, F-91405 Orsay, France.
[Bock, J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Burgarella, D.; Lagache, G.; Alvarez-Marquez, J.] Univ Aix Marseille, LAM, F-13388 Marseille 13, France.
[Burgarella, D.; Lagache, G.; Alvarez-Marquez, J.] CNRS, UMR7326, F-13388 Marseille 13, France.
[Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 1A6, Canada.
[Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA.
[Conversi, L.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, E-28691 Madrid, Spain.
[Duivenvoorden, S.; Oliver, S. J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Dunlop, J. S.; Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Franceschini, A.; Marchetti, L.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Halpern, M.; Marsden, G.; Scott, Douglas] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Magdis, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Perez-Fournon, I.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Perez-Fournon, I.] ULL, Dept Astrofis, E-38205 Tenerife, Spain.
[Schulz, B.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Wang, L.] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands.
[Wang, L.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Wardlow, J.] Univ Copenhagen, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
RP Viero, MP (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 382 Via Pueblo Mall, Stanford, CA 94305 USA.
EM marco.viero@stanford.edu
RI Magdis, Georgios/C-7295-2014; Ivison, R./G-4450-2011;
OI Magdis, Georgios/0000-0002-4872-2294; Ivison, R./0000-0001-5118-1313;
Scott, Douglas/0000-0002-6878-9840; Marchetti,
Lucia/0000-0003-3948-7621; Wardlow, Julie /0000-0003-2376-8971;
Bethermin, Matthieu/0000-0002-3915-2015
FU national funding agency: CSA (Canada); national funding agency: NAOC
(China); national funding agency: CEA (France); national funding agency:
CNES (France); national funding agency: CNRS (France); national funding
agency: ASI (Italy); national funding agency: MCINN (Spain); national
funding agency: SNSB (Sweden); national funding agency: STFC (UK);
national funding agency: UKSA (UK); national funding agency: NASA (USA)
FX M.P.V. warmly thanks Charlotte Clarke, Pete Hurley, Seb Oliver, and the
University of Sussex for their hospitality during the development of
this study, and Phil Hopkins for valuable discussions of the z > 4
universe. We also thank the anonymous referee, whose careful comments
greatly improved this paper. 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 SPIRE data for this paper were obtained as a part of proposal
KPGT_soliver_1, with images made using the following OBSIDs:
1342222819-26, 1342222846-54, 1342222879-80, 1342222897-901.
NR 50
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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 AUG 20
PY 2015
VL 809
IS 2
AR L22
DI 10.1088/2041-8205/809/2/L22
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ6LI
UT WOS:000360715500005
ER
PT J
AU Refaat, TF
Singh, UN
Petros, M
Remus, R
Yu, JR
AF Refaat, Tamer F.
Singh, Upendra N.
Petros, Mulugeta
Remus, Ruben
Yu, Jirong
TI Self-calibration and laser energy monitor validations for a
double-pulsed 2-mu m CO2 integrated path differential absorption lidar
application
SO APPLIED OPTICS
LA English
DT Article
ID SPECTROMETER; SENSITIVITY; SYSTEM
AB Double-pulsed 2-mu m integrated path differential absorption (IPDA) lidar is well suited for atmospheric CO2 remote sensing. The IPDA lidar technique relies on wavelength differentiation between strong and weak absorbing features of the gas normalized to the transmitted energy. In the double-pulse case, each shot of the transmitter produces two successive laser pulses separated by a short interval. Calibration of the transmitted pulse energies is required for accurate CO2 measurement. Design and calibration of a 2-mu m double-pulse laser energy monitor is presented. The design is based on an InGaAs pin quantum detector. A high-speed photoelectromagnetic quantum detector was used for laser-pulse profile verification. Both quantum detectors were calibrated using a reference pyroelectric thermal detector. Calibration included comparing the three detection technologies in the single-pulsed mode, then comparing the quantum detectors in the double-pulsed mode. In addition, a self-calibration feature of the 2-mu m IPDA lidar is presented. This feature allows one to monitor the transmitted laser energy, through residual scattering, with a single detection channel. This reduces the CO2 measurement uncertainty. IPDA lidar ground validation for CO2 measurement is presented for both calibrated energy monitor and self-calibration options. The calibrated energy monitor resulted in a lower CO2 measurement bias, while self-calibration resulted in a better CO2 temporal profiling when compared to the in situ sensor. (C) 2015 Optical Society of America
C1 [Refaat, Tamer F.; Singh, Upendra N.; Petros, Mulugeta; Remus, Ruben; Yu, Jirong] NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Refaat, TF (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA.
EM tamer.f.refaat@nasa.gov
FU NASA Earth Science Technology Office (ESTO ATI-QRS)
FX NASA Earth Science Technology Office (ESTO ATI-QRS-2012).
NR 19
TC 7
Z9 7
U1 2
U2 13
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 AUG 20
PY 2015
VL 54
IS 24
BP 7240
EP 7251
DI 10.1364/AO.54.007240
PG 12
WC Optics
SC Optics
GA CP9CB
UT WOS:000360190200015
PM 26368759
ER
PT J
AU Howard, AM
Nibbelink, N
Bernardes, S
Fragaszy, DM
Maddene, M
AF Howard, Allison M.
Nibbelink, Nathan
Bernardes, Sergio
Fragaszy, Dorothy M.
Maddene, Marguerite
TI Remote sensing and habitat mapping for bearded capuchin monkeys (Sapajus
libidinosus): landscapes for the use of stone tools
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE species distribution model; geographic information system; maximum
entropy modeling; high-resolution imagery; conservation
ID BRAZILIAN CERRADO VEGETATION; MAXENT; CONSERVATION; MODELS; SPACE
AB Application of remote sensing and geographic information systems to the characterization of wildlife habitats is an area of growing significance for conservation. We examine the use of space of a group of bearded capuchin monkeys, a species unique in their use of stone tools to extract encapsulated foods. We define important landscape variables associated with the monkeys' behavior, especially the use of stone tools. Maximum entropy modeling is used to define the landscape characteristics associated with the monkeys' use of space. The variables evaluated in model building include normalized difference vegetation index, distance to roads, distance to areas of human influence, distance to vertical scarps, elevation, land cover/land use class, and percentages of green vegetation, bare soil, and shadow from spectral mixture analysis. Distance to areas of human influence and distance to vertical scarps were the variables most closely associated with capuchin habitat suitability (permutation importance 31.7% and 21%, respectively). Stone tool use occurred in areas of lower elevation and higher percent green vegetation relative to other behavior. These results may inform efforts for conserving the unique stone tool use of this species, especially relevant due to the recent expansion and intensification of industrial agriculture in the region. (C) 2015 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Howard, Allison M.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Nibbelink, Nathan] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA.
[Bernardes, Sergio] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fragaszy, Dorothy M.] Univ Georgia, Dept Psychol, Athens, GA 30602 USA.
[Howard, Allison M.; Bernardes, Sergio; Maddene, Marguerite] Univ Georgia, Ctr Geospatial Res, Dept Geog, Athens, GA 30602 USA.
RP Howard, AM (reprint author), Univ Maryland, Dept Biol, 1210 Biol Psychol Bldg, College Pk, MD 20742 USA.
EM allisonmariehoward@gmail.com
FU NSF ABI grant [1062411]; American Society of Primatologists Small
Research Grant
FX This work was funded by NSF ABI grant 1062411 and the American Society
of Primatologists Small Research Grant. High resolution satellite
imagery was provided by the Intergraph (R) and DigitalGlobe Geospatial
Challenge. We wish to thank Leigh Anna Young for her assistance in
collecting behavioral and positional data in the field. We thank
Caroline Jones for her assistance in collecting data on the spatial
accuracy of the tablet computers at our field site. We thank Marino
Gomes de Oliveira's family for allowing us to conduct our research at
Fazenda Boa Vista. Finally, we thank the EthoCebus Project Research Team
for their collaboration, participation, and support.
NR 34
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U1 3
U2 21
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 1931-3195
J9 J APPL REMOTE SENS
JI J. Appl. Remote Sens.
PD AUG 19
PY 2015
VL 9
AR 096020
DI 10.1117/1.JRS.9.096020
PG 18
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA CP3XV
UT WOS:000359817100001
ER
PT J
AU PopoviC, M
Fliss, PS
Ditzler, MA
AF Popovic, Milena
Fliss, Palmer S.
Ditzler, Mark A.
TI In vitro evolution of distinct self-cleaving ribozymes in diverse
environments
SO NUCLEIC ACIDS RESEARCH
LA English
DT Article
ID THROUGHPUT SEQUENCE-ANALYSIS; GROUP-II INTRON; HAMMERHEAD RIBOZYME;
STRUCTURAL DIVERSITY; ARCHEAN ATMOSPHERE; RNA ENZYME; CATALYSIS; IRON;
PH; EMERGENCE
AB In vitro evolution experiments have long been used to evaluate the roles of RNA in both modern and ancient biology, and as a tool for biotechnology applications. The conditions under which these experiments have been conducted, however, do not reflect the range of cellular environments in modern biology or our understanding of chemical environments on the early earth, when the atmosphere and oceans were largely anoxic and soluble Fe2+ was abundant. To test the impact of environmental factors relevant to RNA's potential role in the earliest forms of life, we evolved populations of self-cleaving ribozymes in an anoxic atmosphere with varying pH in the presence of either Fe2+ or Mg2+. Populations evolved under these different conditions are dominated by different sequences and secondary structures, demonstrating global differences in the underlying fitness landscapes. Comparisons between evolutionary outcomes and catalytic activities also indicate that Mg2+ can readily take the place of Fe2+ in supporting the catalysis of RNA cleavage at neutral pH, but not at lower pH. These results highlight the importance of considering the specific environments in which functional biopolymers evolve when evaluating their potential roles in the origin of life, extant biology, or biotechnology.
C1 [Popovic, Milena] NASA, Ames Res Ctr, Postdoctoral Program, Moffett Field, CA 94035 USA.
[Popovic, Milena; Ditzler, Mark A.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Exobiol Branch, Moffett Field, CA 94035 USA.
[Popovic, Milena; Fliss, Palmer S.] Blue Marble Space Inst Sci, Seattle, WA 98145 USA.
RP Ditzler, MA (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Exobiol Branch, Moffett Field, CA 94035 USA.
EM mark.a.ditzler@nasa.gov
OI Ditzler, Mark /0000-0003-3108-4596
FU Science Innovation Fund Grant; NASA Exobiology Grant; NASA Postdoctoral
Program Fellowship; National Aeronautics and Space Administration
FX Science Innovation Fund Grant and NASA Exobiology Grant from NASA to MAD
and NASA Postdoctoral Program Fellowship to MP. Funding for open access
charge: National Aeronautics and Space Administration.
NR 54
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Z9 4
U1 1
U2 11
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0305-1048
EI 1362-4962
J9 NUCLEIC ACIDS RES
JI Nucleic Acids Res.
PD AUG 18
PY 2015
VL 43
IS 14
BP 7070
EP 7082
DI 10.1093/nar/gkv648
PG 13
WC Biochemistry & Molecular Biology
SC Biochemistry & Molecular Biology
GA CQ4PX
UT WOS:000360588200040
PM 26130717
ER
PT J
AU Romano, JD
Taylor, SR
Cornish, NJ
Gair, J
Mingarelli, CMF
van Haasteren, R
AF Romano, Joseph D.
Taylor, Stephen R.
Cornish, Neil J.
Gair, Jonathan
Mingarelli, Chiara M. F.
van Haasteren, Rutger
TI Phase-coherent mapping of gravitational-wave backgrounds using
ground-based laser interferometers
SO PHYSICAL REVIEW D
LA English
DT Article
AB We extend the formalisms developed in Gair et al. [1] and Cornish and van Haasteren [2] to create maps of gravitational-wave backgrounds using a network of ground-based laser interferometers. We show that in contrast to pulsar timing arrays, which are insensitive to the curl modes of the background, a network of ground-based interferometers is sensitive to both the gradient and curl components. The spatial separation of a network of interferometers, or of a single interferometer at different times during its rotational and orbital motion around the Sun, allows for recovery of both components. We derive expressions for the response functions of a laser interferometer in the small-antenna limit and use these expressions to calculate the overlap reduction function for a pair of interferometers. We also construct maximum-likelihood estimates of the +- and X-polarization modes of the gravitational-wave sky in terms of the response matrix for a network of ground-based interferometers, evaluated at discrete times during Earth's rotational and orbital motion around the Sun. We demonstrate the feasibility of this approach for some simple simulated backgrounds (a single point source and two spatially extended distributions having only gradient or curl components), calculating maximum-likelihood sky maps and uncertainty maps based on the (pseudo) inverse of the response matrix. The distinction between this approach and standard methods for mapping gravitational-wave power is also discussed.
C1 [Romano, Joseph D.] Univ Texas Brownsville, Dept Phys & Astron, Brownsville, TX 78520 USA.
[Romano, Joseph D.] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA.
[Taylor, Stephen R.; van Haasteren, Rutger] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
[Cornish, Neil J.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
[Gair, Jonathan] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Mingarelli, Chiara M. F.] CALTECH, TAPIR, Pasadena, CA 91125 USA.
[Mingarelli, Chiara M. F.] Max Planck Inst Radio Astron, D-53121 Bonn, Germany.
RP Romano, JD (reprint author), Univ Texas Brownsville, Dept Phys & Astron, Brownsville, TX 78520 USA.
OI Taylor, Stephen/0000-0003-0264-1453
FU National Science Foundation [PHY-1205585, PHY-1306702, CREST
HRD-1242090]; NASA [PF3-140116]; NANOGrav Physics Frontier Center [NSF
PFC-1430284]; Royal Society; Marie Curie International Outgoing
Fellowship within the 7th European Community Framework Programme; Higher
Education Funding Council for England; Science and Technology Facilities
Council
FX J. D. R. acknowledges support from National Science Foundation Awards
No. PHY-1205585 and No. CREST HRD-1242090. This research was in part
supported by S. T.'s appointment to the NASA Postdoctoral Program at the
Jet Propulsion Laboratory, administered by Oak Ridge Associated
Universities through a contract with NASA. N. J. C. acknowledges support
from National Science Foundation Award No. PHY-1306702 and the NANOGrav
Physics Frontier Center, Award No. NSF PFC-1430284. J. G.'s work is
supported by the Royal Society. C. M. F. M.'s work is supported by a
Marie Curie International Outgoing Fellowship within the 7th European
Community Framework Programme. R. v. H. acknowledges support by NASA
through Einstein Fellowship Grant No. PF3-140116. J. D. R. thanks Malik
Rakhmanov for useful discussions regarding pseudoinverse calculations
when the system of equations is underdetermined. This research has made
use of PYTHON and its standard libraries: NUMPY and MATPLOTLIB. We have
also made use of MEALPIX (MATLAB implementation of HEALPix [28]),
developed by the GWAstro Research Group and available from
http://gwastro.psu.edu. This work was performed using the Darwin
Supercomputer of the University of Cambridge High Performance Computing
Service (http://www.hpc.cam.ac.uk/), provided by Dell Inc. using
Strategic Research Infrastructure Funding from the Higher Education
Funding Council for England and funding from the Science and Technology
Facilities Council. This paper has been assigned LIGO DCC No.
LIGO-P1500065.
NR 29
TC 2
Z9 2
U1 0
U2 1
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 AUG 18
PY 2015
VL 92
IS 4
AR 042003
DI 10.1103/PhysRevD.92.042003
PG 22
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CP4QH
UT WOS:000359866900001
ER
PT J
AU Burms, J
Caluwaerts, K
Dambre, J
AF Burms, Jeroen
Caluwaerts, Ken
Dambre, Joni
TI Reward-modulated Hebbian plasticity as leverage for partially embodied
control in compliant robotics
SO FRONTIERS IN NEUROROBOTICS
LA English
DT Article
DE compliant robotics; Hebbian plasticity; morphological computation;
recurrent neural networks; tensegrity
ID LEARNING RULE; TENSEGRITY; NETWORKS; NOISE; MODEL
AB In embodied computation (or morphological computation), part of the complexity of motor control is offloaded to the body dynamics. We demonstrate that a simple Hebbian-like learning rule can be used to train systems with (partial) embodiment, and can be extended outside of the scope of traditional neural networks. To this end, we apply the learning rule to optimize the connection weights of recurrent neural networks with different topologies and for various tasks. We then apply this learning rule to a simulated compliant tensegrity robot by optimizing static feedback controllers that directly exploit the dynamics of the robot body. This leads to partially embodied controllers, i.e., hybrid controllers that naturally integrate the computations that are performed by the robot body into a neural network architecture. Our results demonstrate the universal applicability of reward-modulated Hebbian learning. Furthermore, they demonstrate the robustness of systems trained with the learning rule. This study strengthens our belief that compliant robots should or can be seen as computational units, instead of dumb hardware that needs a complex controller. This link between compliant robotics and neural networks is also the main reason for our search for simple universal learning rules for both neural networks and robotics.
C1 [Burms, Jeroen; Caluwaerts, Ken; Dambre, Joni] Univ Ghent, Elect & Informat Syst Dept ELIS, Comp Syst Lab Reservoir Team, B-9000 Ghent, Belgium.
[Caluwaerts, Ken] Oak Ridge Associated Univ, NASA Ames Res Ctr, Intelligent Robot Grp, Moffett Field, CA USA.
RP Dambre, J (reprint author), Sint Pietersnieuwstr 41, Ghent, Belgium.
EM joni.dambre@ugent.be
RI Dambre, Joni/C-2926-2013
OI Dambre, Joni/0000-0002-9373-1210
FU Ph.D. fellowship of Research Foundation - Flanders (FWO); European Union
Seventh Framework Programme (FP7) (Human Brain Project) [248311, 604102]
FX We would like to thank Andrea Soltoggio for useful discussions in the
preparation of this letter. Funding: This research was funded by a Ph.D.
fellowship of the Research Foundation - Flanders (FWO) and the European
Union Seventh Framework Programme (FP7/2007-2013) under grant agreements
No. 248311 (AMARSi), and No. 604102 (Human Brain Project).
NR 30
TC 3
Z9 3
U1 3
U2 7
PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
SN 1662-5218
J9 FRONT NEUROROBOTICS
JI Front. Neurorobotics
PD AUG 17
PY 2015
VL 9
AR 9
DI 10.3389/fnbot.2015.00009
PG 15
WC Computer Science, Artificial Intelligence; Robotics; Neurosciences
SC Computer Science; Robotics; Neurosciences & Neurology
GA DE1RB
UT WOS:000370403000001
PM 26347645
ER
PT J
AU Qiu, SY
Dong, XQ
Xi, B
Li, JLF
AF Qiu, Shaoyue
Dong, Xiquan
Xi, Baike
Li, J. -L. F.
TI Characterizing Arctic mixed-phase cloud structure and its relationship
with humidity and temperature inversion using ARM NSA observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE mixed-phase cloud; humidity inversion; temperature inversion; cloud base
height; cloud occurrence
ID ATMOSPHERIC RADIATION; MICROPULSE LIDAR; CLIMATE RESEARCH; REMOTE
SENSORS; SURFACE; RADAR; STRATOCUMULUS; SENSITIVITY; MOISTURE; PROGRAM
AB In this study, the characteristics of the Arctic mixed-phase cloud (AMC) have been investigated using data collected at the Atmospheric Radiation Measurement North Slope Alaska site from October 2006 to September 2009. AMC has an annual occurrence frequency of 42.3%, which includes 18.7% of single-layered AMCs and 23.6% for multiple layers. Two cloud base heights (CBHs) are defined from ceilometer and micropulse lidar (MPL) measurements. For single-layered AMC, the ceilometer-derived CBH represents the base of the liquid-dominant layer near the cloud top, while MPL-derived CBH represents base of the lower ice-dominant layer. The annual mean CBHs from ceilometer and MPL measurements are 1.0km and 0.6km, respectively, with the largest difference (similar to 1.0km) occurring from December to March and the smallest difference in September. The humidity inversion occurrence decreases with increasing humidity inversion intensity (stronger in summer than in winter). During the winter months, AMC occurrences increase from 15% to 35% when the inversion intensity increases from 0.1 to 0.9g/kg. On the contrary, despite a higher frequency of strong humidity inversion in summer, AMC occurrences are nearly invariant for different inversion intensities. On average, humidity and temperature inversion frequencies of occurrence above an AMC are 5 and 8 times, respectively, as high as those below an AMC. The strong inversion occurrences for both humidity and temperature above an AMC provide the moisture sources from above for the formation and maintenance of AMCs. This result helps to reconcile the persistency of AMCs even when the Arctic surface is covered by snow and ice.
C1 [Qiu, Shaoyue; Dong, Xiquan; Xi, Baike] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58201 USA.
[Li, J. -L. F.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Dong, XQ (reprint author), Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58201 USA.
EM dong@aero.und.edu
OI 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; DOE
ASR project at University of North Dakota [DE-SC0008468]; NASA CERES
project at University of North Dakota [NNX14AP84G]
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. The data can be downloaded from
http://www.archive.arm.gov/. This study was primarily supported by the
DOE ASR project at University of North Dakota with award DE-SC0008468
and the NASA CERES project at University of North Dakota project under
grant NNX14AP84G.
NR 36
TC 3
Z9 3
U1 4
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 AUG 16
PY 2015
VL 120
IS 15
BP 7737
EP 7746
DI 10.1002/2014JD023022
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CQ3KV
UT WOS:000360501900027
ER
PT J
AU Cesana, G
Waliser, DE
Jiang, X
Li, JLF
AF Cesana, G.
Waliser, D. E.
Jiang, X.
Li, J. -L. F.
TI Multimodel evaluation of cloud phase transition using satellite and
reanalysis data
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE GCMs; cloud phase; evaluation; satellite; CALIPSO; multimodel
ID GENERAL-CIRCULATION MODEL; VERTICAL VELOCITY; WATER-CONTENT; CLIMATE;
PRECIPITATION; SIMULATIONS; REPRESENTATION; MICROPHYSICS; VARIABILITY;
SENSITIVITY
AB We take advantage of climate simulations from two multimodel experiments to characterize and evaluate the cloud phase partitioning in 16 general circulation models (GCMs), specifically the vertical structure of the transition between liquid and ice in clouds. We base our analysis on the ratio of ice condensates to the total condensates (phase ratio, PR). Its transition at 90% (PR90) and its links with other relevant variables are evaluated using the GCM-Oriented Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation Cloud Product climatology, reanalysis data, and other satellite observations. In 13 of 16 models, the PR90 transition height occurs too low (6km to 8.4km) and at temperatures too warm (-13.9 degrees C to -32.5 degrees C) compared to observations (8.6km, -33.7 degrees C); features consistent with a lack of supercooled liquid with respect to ice above 6.5km. However, this bias would be slightly reduced by using the lidar simulator. In convective regimes (more humid air and precipitation), the observed cloud phase transition occurs at a warmer temperature than for subsidence regimes (less humid air and precipitation). Only few models manage to roughly replicate the observed correlations with humidity (5/16), vertical velocity (5/16), and precipitation (4/16); 3/16 perform well for all these parameters (MPI-ESM, NCAR-CAM5, and NCHU). Using an observation-based Clausius-Clapeyron phase diagram, we illustrate that the Bergeron-Findeisen process is a necessary condition for models to represent the observed features. Finally, the best models are those that include more complex microphysics.
C1 [Cesana, G.; Waliser, D. E.; Jiang, X.; Li, J. -L. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Jiang, X.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
RP Cesana, G (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Gregory.v.cesana@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. CALIPSO-GOCCP observations were
downloaded from the CFMIP-Observation website
(http://climserv.ipsl.polytechnique.fr/cfmip-obs/Calipso_goccp.html).
ERA-Interim reanalyses were downloaded from ClimServ website
(http://climserv.ipsl.polytechnique.fr/fr/les-donnees/era-interim.html).
GPCP precipitation data were downloaded from
ftp://ftp.cgd.ucar.edu/archive/PRECIP/. The authors thank the climate
modeling groups for producing and making available their model outputs
from the GASS-YoTC/MJOTF and the CMIP5/AMIP experiments. Special thanks
are due to Romain Roehrig (Meteo-France, CNRM-GAME) who provided
CNRM-CM5 outputs using the simulator for Figure 1. The authors also
thank the three anonymous reviewers and the Editor for their relevant
comments, which have improved the manuscript.
NR 80
TC 14
Z9 14
U1 2
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 16
PY 2015
VL 120
IS 15
BP 7871
EP 7892
DI 10.1002/2014JD022932
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA CQ3KV
UT WOS:000360501900034
ER
PT J
AU Chen, Y
Randerson, JT
Morton, DC
AF Chen, Yang
Randerson, James T.
Morton, Douglas C.
TI Tropical North Atlantic ocean-atmosphere interactions synchronize forest
carbon losses from hurricanes and Amazon fires
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE teleconnection; carbon cycle; tropical cyclone; disturbance
ID SEA-SURFACE TEMPERATURE; SOUTH-AMERICA; TREE MORTALITY; CLIMATE;
VARIABILITY; SENSITIVITY; RAINFALL; DIOXIDE; DROUGHT; PRECIPITATION
AB We describe a climate mode synchronizing forest carbon losses from North and South America by analyzing time series of tropical North Atlantic sea surface temperatures (SSTs), landfall hurricanes and tropical storms, and Amazon fires during 1995-2013. Years with anomalously high tropical North Atlantic SSTs during March-June were often followed by a more active hurricane season and a larger number of satellite-detected fires in the southern Amazon during June-November. The relationship between North Atlantic tropical cyclones and southern Amazon fires (r=0.61, p<0.003) was stronger than links between SSTs and either cyclones or fires alone, suggesting that fires and tropical cyclones were directly coupled to the same underlying atmospheric dynamics governing tropical moisture redistribution. These relationships help explain why seasonal outlook forecasts for hurricanes and Amazon fires both failed in 2013 and may enable the design of improved early warning systems for drought and fire in Amazon forests.
C1 [Chen, Yang; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Morton, Douglas C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Chen, Y (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM yang.chen@uci.edu
RI Morton, Douglas/D-5044-2012
FU Gordon and Betty Moore Foundation [GBMF3269]; Regional and Global
Climate Modeling (RGCM) Program in Climate and Environmental Sciences
Division (CESD) of Biological and Environmental Research (BER) Program
in U. S. Dept. of Energy Office of Science; NASA's Terrestrial Ecology
Program
FX We are grateful for the support from the Gordon and Betty Moore
Foundation (GBMF3269), the Regional and Global Climate Modeling (RGCM)
Program in the Climate and Environmental Sciences Division (CESD) of the
Biological and Environmental Research (BER) Program in the U. S. Dept.
of Energy Office of Science, and NASA's Terrestrial Ecology Program.
NR 54
TC 1
Z9 1
U1 6
U2 18
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2015
VL 42
IS 15
BP 6462
EP 6470
DI 10.1002/2015GL064505
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA CQ2FM
UT WOS:000360414900041
ER
PT J
AU Tosca, MG
Diner, DJ
Garay, MJ
Kalashnikova, OV
AF Tosca, M. G.
Diner, D. J.
Garay, M. J.
Kalashnikova, O. V.
TI Human-caused fires limit convection in tropical Africa: First temporal
observations and attribution
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE biomass burning; anthropogenic; Africa; forest fires; smoke; black
carbon
ID COMMUNITY ATMOSPHERE MODEL; CLIMATE SIMULATIONS; CLOUDS; AEROSOLS;
SMOKE; PRECIPITATION; IMPACT; PARAMETERIZATION; INVIGORATION;
CIRCULATION
AB It is well established that smoke particles modify clouds, which in turn affects climate. However, no study has quantified the temporal dynamics of aerosol-cloud interactions with direct observations. Here for the first time, we use temporally offset satellite observations from northern Africa between 2006 and 2010 to quantitatively measure the effect of fire aerosols on convective cloud dynamics. We attribute a reduction in cloud fraction during periods of high aerosol optical depths to a smoke-driven inhibition of convection. We find that higher smoke burdens limit upward vertical motion, increase surface pressure, and increase low-level divergencemeteorological indicators of convective suppression. These results are corroborated by climate simulations that show a smoke-driven increase in regionally averaged shortwave tropospheric heating and decrease in convective precipitation during the fire season. Our results suggest that in tropical regions, anthropogenic fire initiates a positive feedback loop where increased aerosol emissions limit convection, dry the surface, and enable increased fire activity via human ignition.
C1 [Tosca, M. G.; Diner, D. J.; Garay, M. J.; Kalashnikova, O. V.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Tosca, MG (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM michael.g.tosca@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology under a contract with the National Aeronautics
and Space Administration. We thank the MISR team for providing
facilities and useful discussions. We also thank the University of
California, Irvine, and the National Center for Atmospheric Research for
computing facilities. The MISR data were obtained from the NASA Langley
Research Center Atmospheric Science Data Center. The MODIS data were
obtained from the level 1 and Atmosphere Archive and Distribution
System. The ERA-Interim data were obtained from the following
URL:http://apps.ecmwf.int/datasets/.
NR 41
TC 8
Z9 8
U1 3
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 AUG 16
PY 2015
VL 42
IS 15
BP 6492
EP 6501
DI 10.1002/2015GL065063
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA CQ2FM
UT WOS:000360414900045
ER
PT J
AU Carrillo-Sanchez, JD
Plane, JMC
Feng, W
Nesvorny, D
Janches, D
AF Carrillo-Sanchez, J. D.
Plane, J. M. C.
Feng, W.
Nesvorny, D.
Janches, D.
TI On the size and velocity distribution of cosmic dust particles entering
the atmosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE cosmic dust; comets; meteor radar; meteoric ablation; cosmic spherules;
mesospheric metals
ID METEOR OBSERVATIONS; EARTHS ATMOSPHERE; ACCRETION RATE; DEBRIS; RADAR;
CLOUD; MODEL; FLUX; NA
AB The size and velocity distribution of cosmic dust particles entering the Earth's atmosphere is uncertain. Here we show that the relative concentrations of metal atoms in the upper mesosphere, and the surface accretion rate of cosmic spherules, provide sensitive probes of this distribution. Three cosmic dust models are selected as case studies: two are astronomical models, the first constrained by infrared observations of the Zodiacal Dust Cloud and the second by radar observations of meteor head echoes; the third model is based on measurements made with a spaceborne dust detector. For each model, a Monte Carlo sampling method combined with a chemical ablation model is used to predict the ablation rates of Na, K, Fe, Mg, and Ca above 60km and cosmic spherule production rate. It appears that a significant fraction of the cosmic dust consists of small (<5 mu g) and slow (<15 kms(-1)) particles.
C1 [Carrillo-Sanchez, J. D.; Plane, J. M. C.; Feng, W.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England.
[Feng, W.] Univ Leeds, Natl Ctr Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England.
[Nesvorny, D.] Southwest Res Inst, Dept Space Studies, Boulder, CO USA.
[Janches, D.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
RP Plane, JMC (reprint author), Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England.
EM J.M.C.Plane@leeds.ac.uk
RI Janches, Diego/D-4674-2012; Plane, John/C-7444-2015; FENG,
WUHU/B-8327-2008
OI Janches, Diego/0000-0001-8615-5166; Plane, John/0000-0003-3648-6893;
FENG, WUHU/0000-0002-9907-9120
FU European Research Council [291332]; NASA's Solar System Works; NASA
[12-PAST12-0007, 12-PATM12-0006]
FX The data in this paper are available on request from J.M.C.P. This work
is supported by the European Research Council (project 291332 - CODITA).
David Nesvorny has been supported through NASA's Solar System Works.
Diego Janches is supported by NASA awards 12-PAST12-0007 and
12-PATM12-0006.
NR 33
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U1 5
U2 18
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 16
PY 2015
VL 42
IS 15
BP 6518
EP 6525
DI 10.1002/2015GL065149
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA CQ2FM
UT WOS:000360414900048
PM 27478282
ER
PT J
AU Strekalov, DV
Savchenkov, AA
Savchenkova, EA
Matsko, AB
AF Strekalov, Dmitry V.
Savchenkov, Anatoliy A.
Savchenkova, Ekaterina A.
Matsko, Andrey B.
TI Trapping light into high orbital momentum modes of fiber tapers
SO OPTICS LETTERS
LA English
DT Article
ID PHOTONIC CRYSTAL; WAVE-GUIDES; SLOW LIGHT; MICRORESONATORS; RESONATORS;
SOLITONS; CHIP
AB A tapered cylindrical dielectric optical waveguide acts as a high quality factor white-light cavity providing high field concentration as well as long optical group delay. It is possible to optimize shape of a lossless taper to suppress reflection of the input light and to achieve infinitely high field concentration. These tapers can be used in sensing and optoelectronics applications instead of conventional microcavities.
C1 [Strekalov, Dmitry V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Savchenkov, Anatoliy A.; Savchenkova, Ekaterina A.; Matsko, Andrey B.] OEwaves Inc, Pasadena, CA 91107 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
FU California Institute of Technology
FX California Institute of Technology.
NR 29
TC 1
Z9 1
U1 4
U2 10
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 AUG 15
PY 2015
VL 40
IS 16
BP 3782
EP 3785
DI 10.1364/OL.40.003782
PG 4
WC Optics
SC Optics
GA CP2SQ
UT WOS:000359727800026
PM 26274659
ER
PT J
AU Hofmann, DC
Roberts, SN
Kozachkov, H
AF Hofmann, Douglas C.
Roberts, Scott N.
Kozachkov, Henry
TI Infrared thermal processing history of a Ti-based bulk metallic glass
matrix composite manufactured via semi-solid forging
SO ACTA MATERIALIA
LA English
DT Article
DE Bulk metallic glass matrix composites; Thermal imaging; Forging
ID TENSILE DUCTILITY; TRANSFORMATION
AB A method for using non-contact infrared thermal imaging for determining the processing history of bulk metallic glass matrix composites (BMGMCs) during semi-solid forging is presented. The technique allows for the first estimations of the relevant parameters associated with semi-solid forging, including the heating profile, forging temperatures, cooling rates, and formability parameters. The processing parameters are correlated with microstructure and a new forging viscosity estimation is developed and compared with other techniques. The research offers a new strategy for thermal measurements that is widely applicable to other manufacturing processes. (C) 2015 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Hofmann, Douglas C.] CALTECH, Jet Prop Lab, Mat Dev & Mfg Technol Grp, Pasadena, CA 91125 USA.
CALTECH, Keck Lab Engn Sci, Pasadena, CA 91125 USA.
RP Hofmann, DC (reprint author), CALTECH, Jet Prop Lab, Mat Dev & Mfg Technol Grp, Pasadena, CA 91125 USA.
EM dch@jpl.nasa.gov
FU Air Force Office of Scientific Research, United States
[FA9550-12-1-0059]; Presidential Early Career Award; National
Aeronautics and Space Administration
FX This work was funded by the Air Force Office of Scientific Research,
United States, under grant number FA9550-12-1-0059. D.C.H. also cites
partial funding from the Presidential Early Career Award. The authors
thank Georg Kaltenboeck for useful discussions. 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 37
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U1 4
U2 32
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6454
EI 1873-2453
J9 ACTA MATER
JI Acta Mater.
PD AUG 15
PY 2015
VL 95
BP 192
EP 200
DI 10.1016/j.actamat.2015.05.029
PG 9
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA CN7PJ
UT WOS:000358626200021
ER
PT J
AU Hernandez, D
Cabrera, CR
Mendez, L
Diaz-Serrano, M
Vega, O
Weiner, BR
Rosa, LG
AF Hernandez, Dionne
Cabrera, Carlos R.
Mendez, Laura
Diaz-Serrano, Madeline
Vega, Omar
Weiner, Brad R.
Rosa, Luis G.
TI Oxidized SWCNT chemically attached to a modified copper substrate
SO APPLIED SURFACE SCIENCE
LA English
DT Article
DE Single-wall carbon nanotubes; Copper substrate; Surface modification;
Self-assembly monolayer; 4-Aminothiophenol; Chemical attachment
ID SELF-ASSEMBLED MONOLAYERS; WALLED CARBON NANOTUBES; ELECTRODES
AB Oxidized single-wall carbon nanotubes were chemically attached to a modified copper substrate by means of a 4-aminothiophenol (4-ATP) self-assembly monolayer (SAM). This bottom up approach offers a low cost route to attach carbon nanotubes by using a condensation reaction. Here, the exposed amine from the 4-ATP SAM reacts with the carboxylic group (COOH) on the CNT. The reaction was followed using ATR-FTIR and the surface was characterized using SEM, XPS, and Raman. The analytical techniques used on this study suggest that the condensation reaction employed using a carbodiimide such as 1-Ethyl-3-[3-dimethylaminopropyl] carbodiimide hydrochloride (EDC) produced SWCNT attached to the copper substrate. Published by Elsevier B.V.
C1 [Hernandez, Dionne; Cabrera, Carlos R.; Diaz-Serrano, Madeline; Weiner, Brad R.] Univ Puerto Rico, Dept Chem, San Juan, PR 00931 USA.
[Mendez, Laura] Univ Puerto Rico, Dept Phys, San Juan, PR 00936 USA.
[Hernandez, Dionne; Mendez, Laura; Weiner, Brad R.; Rosa, Luis G.] Univ Puerto Rico, Inst Funct Nanomat, San Juan, PR 00931 USA.
[Cabrera, Carlos R.] Univ Puerto Rico, Ctr Adv Nanoscale Mat, San Juan, PR 00936 USA.
[Vega, Omar; Rosa, Luis G.] Univ Puerto Rico Humacao, Dept Phys & Elect, Humacao, PR 00791 USA.
RP Hernandez, D (reprint author), NASA Glenn Res Ctr, LEXPhotovolta & Electrochem Branch, 21000 Brookpark Rd,Mail Stop 309-1, Cleveland, OH 44135 USA.
EM dmhernandezlugo@gmail.com
OI Cabrera, Carlos/0000-0002-3342-8666
FU NASA Harriet-Jenkins Pre-docotoral Program [NNX10AU20A]; Institute for
Functional Nanomaterials (NSF) [1002410]; PR NASA EPSCoR [NNX13AB22A];
PR NASA Space Grant [NNX10AM80H]; NASA-URC Center for Advance Nanoscale
Materials [NNX08BA48A]
FX Dionne Hernandez-Lugo gratefully acknowledges the financial support from
NASA Harriet-Jenkins Pre-docotoral Program (Grant No. NNX10AU20A). This
research project was carried out under the auspices of the Institute for
Functional Nanomaterials (NSF Grant No. 1002410). This research was also
supported in part by PR NASA EPSCoR (NNX13AB22A) and PR NASA Space Grant
(NNX10AM80H) and the NASA-URC Center for Advance Nanoscale Materials
((NNX08BA48A) The authors gratefully acknowledge the instrumentation and
technical support of the Materials Characterization Center of the
University of Puerto Rico for the XPS (Dr. E. Facchini), the Raman
Facility (Dr. R.S. Katiyar). Also we will like to thank Dr. Diana
Santiago for ATR-FTIR analysis at NASA Glenn Research Center.
NR 17
TC 1
Z9 1
U1 3
U2 44
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-4332
EI 1873-5584
J9 APPL SURF SCI
JI Appl. Surf. Sci.
PD AUG 15
PY 2015
VL 346
BP 415
EP 422
DI 10.1016/j.apsusc.2015.02.194
PG 8
WC Chemistry, Physical; Materials Science, Coatings & Films; Physics,
Applied; Physics, Condensed Matter
SC Chemistry; Materials Science; Physics
GA CI8IW
UT WOS:000355017000055
ER
PT J
AU Hornbuckle, BC
Noebe, RD
Thompson, GB
AF Hornbuckle, B. C.
Noebe, R. D.
Thompson, G. B.
TI Influence of Hf solute additions on the precipitation and hardenability
in Ni-rich NiTi alloys
SO JOURNAL OF ALLOYS AND COMPOUNDS
LA English
DT Article
DE NiTi; Hardness; Precipitate strengthening; TEM
ID SHAPE-MEMORY ALLOYS; MARTENSITIC-TRANSFORMATION; PHASE; NI4TI3
AB Very Ni-rich NiTi alloys have recently been shown to have an unusually high hardness, comparable to tool steels, and other attributes that make them promising candidates for bearing and related applications. This high hardness has been associated with the precipitation of a large volume fraction of Ni4Ti3 platelets, resulting in a matrix that consists of narrow B2 matrix channels. In this work, a series of Ni-rich ternary alloys with dilute solute additions of Hf (54Ni-45Ti-1Hf, 55Ni-44Ti-1Hf, 54Ni-44Ti-2Hf, and 56Ni-40Ti-4Hf (at.%)) have been investigated. Transmission electron microscopy confirmed a B2 NiTi matrix phase containing nanoscale Ni4Ti3 platelets, H-phase precipitates, and R-phase; however, the H-phase and R-phase were not present initially but only after aging for a period of time. At aging times greater than similar to 100 h at 400 degrees C, all ternary alloys showed a slight secondary increase in hardness, which was attributed to H-phase precipitation and growth within the B2 channels. In the particular case of the 56Ni-40Ti-4Hf alloy, hardness increased with aging to a maximum value of 679 VHN, which was greater than all other binary or ternary alloys examined. Additionally the H-phase appeared to alter or delay the typical breakdown sequence of the metastable Ni4Ti3 strengthening phase by removing the excess Ni needed for its decomposition. The collective results provide new material insights for creating a next-generation NiTi based bearing alloy. (C) 2015 Elsevier B.V. All rights reserved.
C1 [Hornbuckle, B. C.; Thompson, G. B.] Univ Alabama, Dept Met & Mat Engn, Tuscaloosa, AL 35487 USA.
[Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA.
RP Thompson, GB (reprint author), Univ Alabama, Dept Met & Mat Engn, Tuscaloosa, AL 35487 USA.
EM gthompson@eng.ua.edu
FU NASA [NNX09AO61A]; NASA Transformative Aeronautics Concepts Program,
Transformation Tools & Technologies Project (Dale Hopkins, Technical
Lead for Structure & Materials Discipline)
FX The authors gratefully acknowledge funding for this research under NASA
grant NNX09AO61A and from the NASA Transformative Aeronautics Concepts
Program, Transformation Tools & Technologies Project (Dale Hopkins,
Technical Lead for Structure & Materials Discipline). UA's Central
Analytical Facility (www.caf.ua.edu) is recognized for additional
support and access to the microscopes used in this study.
NR 19
TC 0
Z9 0
U1 6
U2 16
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0925-8388
EI 1873-4669
J9 J ALLOY COMPD
JI J. Alloy. Compd.
PD AUG 15
PY 2015
VL 640
BP 449
EP 454
DI 10.1016/j.jallcom.2015.04.002
PG 6
WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy &
Metallurgical Engineering
SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering
GA CH7DK
UT WOS:000354195600069
ER
PT J
AU Brehm, C
Hader, C
Fasel, HF
AF Brehm, C.
Hader, C.
Fasel, H. F.
TI A locally stabilized immersed boundary method for the compressible
Navier-Stokes equations
SO JOURNAL OF COMPUTATIONAL PHYSICS
LA English
DT Article
DE Immersed boundary; Higher-order finite-difference; Numerical stability
analysis; Compressible flows
ID CARTESIAN GRID METHOD; LOW REYNOLDS NUMBERS; CIRCULAR-CYLINDER;
INCOMPRESSIBLE FLOWS; NUMERICAL-SIMULATION; ELLIPTIC-EQUATIONS;
INTERFACE METHOD; VISCOUS-FLOW; STEADY FLOW; SCHEMES
AB A higher-order immersed boundary method for solving the compressible Navier-Stokes equations is presented. The distinguishing feature of this new immersed boundary method is that the coefficients of the irregular finite-difference stencils in the vicinity of the immersed boundary are optimized to obtain improved numerical stability. This basic idea was introduced in a previous publication by the authors for the advection step in the projection method used to solve the incompressible Navier-Stokes equations. This paper extends the original approach to the compressible Navier-Stokes equations considering flux vector splitting schemes and viscous wall boundary conditions at the immersed geometry. In addition to the stencil optimization procedure for the convective terms, this paper discusses other key aspects of the method, such as imposing flux boundary conditions at the immersed boundary and the discretization of the viscous flux in the vicinity of the boundary. Extensive linear stability investigations of the immersed scheme confirm that a linearly stable method is obtained. The method of manufactured solutions is used to validate the expected higher-order accuracy and to study the error convergence properties of this new method. Steady and unsteady, 2D and 3D canonical test cases are used for validation of the immersed boundary approach. Finally, the method is employed to simulate the laminar to turbulent transition process of a hypersonic Mach 6 boundary layer flow over a porous wall and subsonic boundary layer flow over a three-dimensional spherical roughness element. (C) 2015 Elsevier Inc. All rights reserved.
C1 [Brehm, C.] NASA Ames, Sci & Technol Corp, Moffett Field, CA 94035 USA.
[Hader, C.; Fasel, H. F.] Univ Arizona, Tucson, AZ USA.
RP Brehm, C (reprint author), NASA Ames, Sci & Technol Corp, Moffett Field, CA 94035 USA.
EM christoph.brehm@nasa.gov
OI Brehm, Christoph/0000-0002-9006-3587
FU Applied Modeling Simulation Branch at NASA ARC; Hypersonic Center for
Laminar Turbulent Transition Research
FX The authors gratefully acknowledge the contributions from the LAVA group
at Applied Modeling Simulation Branch NASA Ames Research Center (ARC).
The work was partially funded by the Applied Modeling Simulation Branch
at NASA ARC and the Hypersonic Center for Laminar Turbulent Transition
Research.
NR 54
TC 5
Z9 5
U1 4
U2 29
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0021-9991
EI 1090-2716
J9 J COMPUT PHYS
JI J. Comput. Phys.
PD AUG 15
PY 2015
VL 295
BP 475
EP 504
DI 10.1016/j.jcp.2015.04.023
PG 30
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA CI0BD
UT WOS:000354399700023
ER
PT J
AU Tinto, M
Yu, N
AF Tinto, Massimo
Yu, Nan
TI Time-delay interferometry with optical frequency comb
SO PHYSICAL REVIEW D
LA English
DT Article
ID NOBEL LECTURE; SPACE; LASER; STABILITY; PRECISION
AB Heterodyne laser phase measurements in a space-based gravitational wave interferometer are degraded by the phase fluctuations of the onboard clocks, resulting in unacceptable sensitivity performance levels of the interferometric data. In order to calibrate out the clock phase noises, it has previously been suggested that additional interspacecraft phase measurements must be performed by modulating the laser beams. With the advent of self-referenced optical frequency combs, it is possible to generate a heterodyne microwave signal that is coherently referenced to the onboard laser. We show in this case that the microwave noise can be canceled directly by applying modified second-generation time-delay interferometric combinations to the heterodyne phase measurements. This approach avoids the use of modulated laser beams as well as the need for additional ultrastable oscillator clocks.
C1 [Tinto, Massimo; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tinto, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Massimo.Tinto@jpl.nasa.gov; Nan.Yu@jpl.nasa.gov
FU Jet Propulsion Laboratory Research and Technology Development Program
FX We acknowledge financial support provided by the Jet Propulsion
Laboratory Research and Technology Development Program. This research
was performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration.
NR 32
TC 1
Z9 1
U1 11
U2 20
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 AUG 14
PY 2015
VL 92
IS 4
AR 042002
DI 10.1103/PhysRevD.92.042002
PG 12
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA CO9IT
UT WOS:000359489300001
ER
PT J
AU Mahnert, A
Vaishampayan, P
Probst, AJ
Auerbach, A
Moissl-Eichinger, C
Venkateswaran, K
Berg, G
AF Mahnert, Alexander
Vaishampayan, Parag
Probst, Alexander J.
Auerbach, Anna
Moissl-Eichinger, Christine
Venkateswaran, Kasthuri
Berg, Gabriele
TI Cleanroom Maintenance Significantly Reduces Abundance but Not Diversity
of Indoor Microbiomes
SO PLOS ONE
LA English
DT Article
ID PROPIDIUM MONOAZIDE; GENE-SEQUENCES; SPACECRAFT; ENVIRONMENT; BACTERIAL;
COMMUNITIES; PRIMERS; ROOM; MICROORGANISMS; COLLECTION
AB Cleanrooms have been considered microbially-reduced environments and are used to protect human health and industrial product assembly. However, recent analyses have deciphered a rather broad diversity of microbes in cleanrooms, whose origin as well as physiological status has not been fully understood. Here, we examined the input of intact microbial cells from a surrounding built environment into a spacecraft assembly cleanroom by applying a molecular viability assay based on propidium monoazide (PMA). The controlled cleanroom (CCR) was characterized by similar to 6.2*10(3) 16S rRNA gene copies of intact bacterial cells per m(2) floor surface, which only represented 1% of the total community that could be captured via molecular assays without viability marker. This was in contrast to the uncontrolled adjoining facility (UAF) that had 12 times more living bacteria. Regarding diversity measures retrieved from 16S rRNA Illumina-tag analyzes, we observed, however, only a minor drop in the cleanroom facility allowing the conclusion that the number but not the diversity of microbes is strongly affected by cleaning procedures. Network analyses allowed tracking a substantial input of living microbes to the cleanroom and a potential enrichment of survival specialists like bacterial spore formers and archaeal halophiles and mesophiles. Moreover, the cleanroom harbored a unique community including 11 exclusive genera, e.g., Haloferax and Sporosarcina, which are herein suggested as indicators of cleanroom environments. In sum, our findings provide evidence that archaea are alive in cleanrooms and that cleaning efforts and cleanroom maintenance substantially decrease the number but not the diversity of indoor microbiomes.
C1 [Mahnert, Alexander; Berg, Gabriele] Graz Univ Technol, Inst Environm Biotechnol, A-8010 Graz, Austria.
[Mahnert, Alexander; Vaishampayan, Parag; Venkateswaran, Kasthuri] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA USA.
[Probst, Alexander J.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Auerbach, Anna; Moissl-Eichinger, Christine] Univ Regensburg, Inst Microbiol, D-93053 Regensburg, Germany.
[Auerbach, Anna; Moissl-Eichinger, Christine] Univ Regensburg, Archaea Ctr, D-93053 Regensburg, Germany.
[Moissl-Eichinger, Christine] Med Univ Graz, Dept Internal Med, Graz, Austria.
[Moissl-Eichinger, Christine] BioTechMed Graz, Graz, Austria.
RP Berg, G (reprint author), Graz Univ Technol, Inst Environm Biotechnol, A-8010 Graz, Austria.
EM gabriele.berg@tugraz.at
RI Probst, Alexander/K-2813-2016
FU BioTechMed-Graz
FX The study was funded by BioTechMed-Graz.
NR 58
TC 6
Z9 6
U1 3
U2 8
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 AUG 14
PY 2015
VL 10
IS 8
AR e0134848
DI 10.1371/journal.pone.0134848
PG 20
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CO9KD
UT WOS:000359493600042
PM 26273838
ER
PT J
AU Famiglietti, JS
Cazenave, A
Eicker, A
Reager, JT
Rodell, M
Velicogna, I
AF Famiglietti, J. S.
Cazenave, A.
Eicker, A.
Reager, J. T.
Rodell, M.
Velicogna, I.
TI Satellites provide the big picture
SO SCIENCE
LA English
DT Editorial Material
ID WATER; MISSION
C1 [Famiglietti, J. S.; Reager, J. T.; Velicogna, I.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
[Famiglietti, J. S.; Velicogna, I.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
[Famiglietti, J. S.] Univ Calif Irvine, Dept Civil & Environm Engn, Irvine, CA USA.
[Cazenave, A.] CNES LEGOS, Toulouse, France.
[Cazenave, A.] Int Space Sci Inst, Bern, Switzerland.
[Eicker, A.] Univ Bonn, Inst Geodesy & Geoinformat, Bonn, Germany.
[Rodell, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Famiglietti, JS (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA.
EM james.famiglietti@jpl.nasa.gov
RI Eicker, Annette/B-6076-2014; Rodell, Matthew/E-4946-2012
OI Eicker, Annette/0000-0002-9087-1445; Rodell, Matthew/0000-0003-0106-7437
NR 20
TC 15
Z9 15
U1 3
U2 33
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD AUG 14
PY 2015
VL 349
IS 6249
BP 684
EP 685
DI 10.1126/science.aac9238
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA CO8JO
UT WOS:000359415100013
PM 26273037
ER
PT J
AU Andersen, KG
Shapiro, BJ
Matranga, CB
Sealfon, R
Lin, AE
Moses, LM
Folarin, OA
Goba, A
Odia, I
Ehiane, PE
Momoh, M
England, EM
Winnicki, S
Branco, LM
Gire, SK
Phelan, E
Tariyal, R
Tewhey, R
Omoniwa, O
Fullah, M
Fonnie, R
Fonnie, M
Kanneh, L
Jalloh, S
Gbakie, M
Saffa, S
Karbo, K
Gladden, AD
Qu, J
Stremlau, M
Nekoui, M
Finucane, HK
Tabrizi, S
Vitti, JJ
Birren, B
Fitzgerald, M
McCowan, C
Ireland, A
Berlin, AM
Bochicchio, J
Tazon-Vega, B
Lennon, NJ
Ryan, EM
Bjornson, Z
Milner, DA
Lukens, AK
Broodie, N
Rowland, M
Heinrich, M
Akdag, M
Schieffelin, JS
Levy, D
Akpan, H
Bausch, DG
Rubins, K
McCormick, JB
Lander, ES
Gunther, S
Hensley, L
Okogbenin, S
Schaffner, SF
Okokhere, PO
Khan, SH
Grant, DS
Akpede, GO
Asogun, DA
Gnirke, A
Levin, JZ
Happi, CT
Garry, RF
Sabeti, PC
AF Andersen, Kristian G.
Shapiro, B. Jesse
Matranga, Christian B.
Sealfon, Rachel
Lin, Aaron E.
Moses, Lina M.
Folarin, Onikepe A.
Goba, Augustine
Odia, Ikponmwonsa
Ehiane, Philomena E.
Momoh, Mambu
England, Eleina M.
Winnicki, Sarah
Branco, Luis M.
Gire, Stephen K.
Phelan, Eric
Tariyal, Ridhi
Tewhey, Ryan
Omoniwa, Omowunmi
Fullah, Mohammed
Fonnie, Richard
Fonnie, Mbalu
Kanneh, Lansana
Jalloh, Simbirie
Gbakie, Michael
Saffa, Sidiki
Karbo, Kandeh
Gladden, Adrianne D.
Qu, James
Stremlau, Matthew
Nekoui, Mahan
Finucane, Hilary K.
Tabrizi, Shervin
Vitti, Joseph J.
Birren, Bruce
Fitzgerald, Michael
McCowan, Caryn
Ireland, Andrea
Berlin, Aaron M.
Bochicchio, James
Tazon-Vega, Barbara
Lennon, Niall J.
Ryan, Elizabeth M.
Bjornson, Zach
Milner, Danny A., Jr.
Lukens, Amanda K.
Broodie, Nisha
Rowland, Megan
Heinrich, Megan
Akdag, Marjan
Schieffelin, John S.
Levy, Danielle
Akpan, Henry
Bausch, Daniel G.
Rubins, Kathleen
McCormick, Joseph B.
Lander, Eric S.
Guenther, Stephan
Hensley, Lisa
Okogbenin, Sylvanus
Schaffner, Stephen F.
Okokhere, Peter O.
Khan, S. Humarr
Grant, Donald S.
Akpede, George O.
Asogun, Danny A.
Gnirke, Andreas
Levin, Joshua Z.
Happi, Christian T.
Garry, Robert F.
Sabeti, Pardis C.
CA Viral Hemorrhagic Fever Consortium
TI Clinical Sequencing Uncovers Origins and Evolution of Lassa Virus
SO CELL
LA English
DT Article
ID WEST-AFRICA; CODON USAGE; PURIFYING SELECTION; DENGUE VIRUS; L-RNA;
FEVER; BIAS; ADAPTATION; ANCIENT; EBOLA
AB The 2013-2015 West African epidemic of Ebola virus disease (EVD) reminds us of how little is known about biosafety level 4 viruses. Like Ebola virus, Lassa virus (LASV) can cause hemorrhagic fever with high case fatality rates. We generated a genomic catalog of almost 200 LASV sequences from clinical and rodent reservoir samples. We show that whereas the 2013-2015 EVD epidemic is fueled by human-to-human transmissions, LASV infections mainly result from reservoir-to-human infections. We elucidated the spread of LASV across West Africa and show that this migration was accompanied by changes in LASV genome abundance, fatality rates, codon adaptation, and translational efficiency. By investigating intrahost evolution, we found that mutations accumulate in epitopes of viral surface proteins, suggesting selection for immune escape. This catalog will serve as a foundation for the development of vaccines and diagnostics.
C1 [Andersen, Kristian G.; Shapiro, B. Jesse; Lin, Aaron E.; Winnicki, Sarah; Gire, Stephen K.; Tewhey, Ryan; Stremlau, Matthew; Nekoui, Mahan; Tabrizi, Shervin; Vitti, Joseph J.; Sabeti, Pardis C.] Harvard Univ, Dept Organism & Evolutionary Biol, FAS Ctr Syst Biol, Cambridge, MA 02138 USA.
[Andersen, Kristian G.; Shapiro, B. Jesse; Matranga, Christian B.; Sealfon, Rachel; Lin, Aaron E.; England, Eleina M.; Winnicki, Sarah; Gire, Stephen K.; Phelan, Eric; Tariyal, Ridhi; Tewhey, Ryan; Gladden, Adrianne D.; Qu, James; Stremlau, Matthew; Nekoui, Mahan; Finucane, Hilary K.; Tabrizi, Shervin; Birren, Bruce; Fitzgerald, Michael; McCowan, Caryn; Ireland, Andrea; Berlin, Aaron M.; Bochicchio, James; Tazon-Vega, Barbara; Lennon, Niall J.; Ryan, Elizabeth M.; Lander, Eric S.; Schaffner, Stephen F.; Gnirke, Andreas; Levin, Joshua Z.; Sabeti, Pardis C.] Broad Inst, Cambridge, MA 02142 USA.
[Andersen, Kristian G.] Scripps Translat Sci Inst, Scripps Res Inst, La Jolla, CA 92037 USA.
[Shapiro, B. Jesse] Univ Montreal, Dept Biol Sci, Montreal, PQ H2V 2S9, Canada.
[Sealfon, Rachel] MIT, Comp Sci & Artificial Intelligence Lab, Cambridge, MA 02139 USA.
[Moses, Lina M.; Schieffelin, John S.; Levy, Danielle; Bausch, Daniel G.; Garry, Robert F.] Tulane Univ, Tulane Hlth Sci Ctr, New Orleans, LA 70118 USA.
[Folarin, Onikepe A.; Odia, Ikponmwonsa; Ehiane, Philomena E.; Omoniwa, Omowunmi; Okogbenin, Sylvanus; Okokhere, Peter O.; Akpede, George O.; Asogun, Danny A.; Happi, Christian T.] Irrua Specialist Teaching Hosp, Inst Lassa Fever Res & Control, Irrua, Edo State, Nigeria.
[Folarin, Onikepe A.; Happi, Christian T.] Redeemers Univ, Coll Nat Sci, Dept Biol Sci, Redemption City, Osun State, Nigeria.
[Goba, Augustine; Momoh, Mambu; Fullah, Mohammed; Fonnie, Richard; Fonnie, Mbalu; Kanneh, Lansana; Jalloh, Simbirie; Gbakie, Michael; Saffa, Sidiki; Karbo, Kandeh; Khan, S. Humarr; Grant, Donald S.] Kenema Govt Hosp, Lassa Fever Lab, Kenema, Eastern Provinc, Sierra Leone.
[Momoh, Mambu; Fullah, Mohammed] Eastern Polytech Coll, Kenema, Eastern Provinc, Sierra Leone.
[Branco, Luis M.; Rowland, Megan; Heinrich, Megan; Akdag, Marjan] Zalgen Labs, Germantown, MD 20876 USA.
[Bjornson, Zach] Stanford Univ, Sch Med, Dept Microbiol & Immunol, Stanford, CA 94304 USA.
[Milner, Danny A., Jr.; Lukens, Amanda K.; Sabeti, Pardis C.] Harvard Univ, Sch Publ Hlth, Dept Immunol & Infect Dis, Boston, MA 02115 USA.
[Broodie, Nisha] Columbia Univ, Coll Med, New York, NY 10032 USA.
[Akpan, Henry] Nigerian Fed Minist Hlth, Abuja, Fed Capital Ter, Nigeria.
[Rubins, Kathleen] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[McCormick, Joseph B.] Univ Texas Sch Publ Hlth, Brownsville, TX 77030 USA.
[Guenther, Stephan] Bernhard Nocht Inst Trop Med, Dept Virol, D-20259 Hamburg, Germany.
[Hensley, Lisa] NIAID Integrated Res Facil, Frederick, MD 21702 USA.
[Viral Hemorrhagic Fever Consortium] Tulane Univ, New Orleans, LA 70118 USA.
RP Sabeti, PC (reprint author), Harvard Univ, Dept Organism & Evolutionary Biol, FAS Ctr Syst Biol, Cambridge, MA 02138 USA.
RI Tazon Vega, Barbara/J-6739-2015; Schaffner, Stephen/D-1189-2011;
OI Tazon Vega, Barbara/0000-0003-4513-5104; Shapiro, B.
Jesse/0000-0001-6819-8699; Broodie, Nisha/0000-0001-6911-328X
FU NIH; Department of Health and Human Services [1DP2OD006514-01]; NIAID
[HHSN272200900049C, HHSN272201000022C, HHSN272200900018C, U19AI110818];
USAMRAA [W81XWH-10-1-0098]; Packard Foundation Fellowship for Science
and Engineering; Broad Institute SPARC award; German Research Foundation
[GU 883/1-1]; Carlsberg Foundation; Harvard MIDAS CCDD postdoctoral
fellowship; Canada Research Chair; NSF [DGE 1122374, 1144152]
FX The authors thank C. Edwards, X. Yang, M. Zody, B. Han, A. Andersen, I.
Shlyakhter, D. Park, M. Henn, M. Busby, M. Kellis, C. Bishop, A.
Haislip, L. Burchfield, A. Matthews, and F. Viloria for their help and
advice. We also thank the Ministry of Health and Sanitation Government
of Sierra Leone, Oyo State Ministry of Health, and the Federal Ministry
of Health, Nigeria. A full list of members of the Viral Hemorrhagic
Fever Consortium can be found at www.vhfc.org. This project was funded
with federal funds from the NIH, Department of Health and Human Services
(1DP2OD006514-01) and NIAID Contracts (HHSN272200900049C,
HHSN272201000022C, HHSN272200900018C, and U19AI110818). The authors
received additional support from USAMRAA (W81XWH-10-1-0098), a Packard
Foundation Fellowship for Science and Engineering, a Broad Institute
SPARC award, and the German Research Foundation (GU 883/1-1). K.G.A. was
supported by a fellowship from the Carlsberg Foundation; B.J.S. was
supported by a Harvard MIDAS CCDD postdoctoral fellowship and Canada
Research Chair; and R.S. and A.E.L. received NSF GRFP fellowships (DGE
1122374 and 1144152). Tulane University and industry partners have filed
patent applications for several Lassa-related technologies and may
receive royalties or profits if commercial products are developed.
NR 51
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PU CELL PRESS
PI CAMBRIDGE
PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA
SN 0092-8674
EI 1097-4172
J9 CELL
JI Cell
PD AUG 13
PY 2015
VL 162
IS 4
BP 738
EP 750
DI 10.1016/j.cell.2015.07.020
PG 13
WC Biochemistry & Molecular Biology; Cell Biology
SC Biochemistry & Molecular Biology; Cell Biology
GA CP2XP
UT WOS:000359741400009
PM 26276630
ER
PT J
AU Yoonessi, M
Lerch, BA
Peck, JA
Rogers, RB
Sola-Lopez, FJ
Meador, MA
AF Yoonessi, Mitra
Lerch, Bradley A.
Peck, John A.
Rogers, Richard B.
Sola-Lopez, Francisco J.
Meador, Michael A.
TI Self-Healing of Core-Shell Magnetic Polystyrene Nanocomposites
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE magnetic polymer nanocomposite; magnetic nanoparticles; self-healing;
smart polymers; polystyrene
ID THERMAL-DEGRADATION; NANOPARTICLES; POLYMER; RESTORATION; NETWORKS
AB High heat generation is reported in core shell magnetic nanoparticle polystyrene (PS) nanocomposites (3.5, 10 wt %) when they are placed in a high-frequency ac magnetic field. These magnetic nanoparticles with cobalt iron oxide core and manganese iron oxide shell were synthesized and characterized by wide-angle X-ray scattering (WAX), thermal gravimetric analysis (TGA), transmission electron microscopy (TEM), and ac field gradient magnetometery. When placed in a high-frequency ac magnetic field, the thermal energy generated in the magnetic polystyrene nanocomposites resulted in a surface temperature increase. The heat generation is attributed to the contribution of Neel relaxation and hysteresis of the core shell magnetic nanoparticles in the solid state. The maximum surface temperature increased with increasing nanoparticle content and resulted in melting of the magnetic polystyrene nanocomposite.
C1 [Yoonessi, Mitra] Ohio Aerosp Inst, Cleveland, OH 44135 USA.
[Lerch, Bradley A.; Rogers, Richard B.; Sola-Lopez, Francisco J.; Meador, Michael A.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Peck, John A.] Univ Akron, Dept Geosci, Akron, OH 44325 USA.
RP Yoonessi, M (reprint author), Ohio Aerosp Inst, Cleveland, OH 44135 USA.
EM mitra.yoonessi@gmail.com
FU NASA Center Innovation Fund program; NASA Structure and Materials
Division; Subsonics Fixed Wing Project; NASA [NNC07BA13B]
FX The NASA Center Innovation Fund program and Structure and Materials
Division are thanked for funding this project. Subsonics Fixed Wing
Project, Fundamental Aeronautics Program (NASA Contract NNC07BA13B),
NASA Center Innovation Fund Program, and Dr. Roshanak Hakimzadeh are
thanked for funding and support of this research. Daniel A. Scheiman is
thanked for the laboratory support.
NR 30
TC 2
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U1 8
U2 59
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1944-8244
J9 ACS APPL MATER INTER
JI ACS Appl. Mater. Interfaces
PD AUG 12
PY 2015
VL 7
IS 31
BP 16932
EP 16937
DI 10.1021/acsami.5b04314
PG 6
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA CP2BX
UT WOS:000359683600006
PM 26192341
ER
PT J
AU Shelhamer, M
AF Shelhamer, Mark
TI Trends in sensorimotor research and countermeasures for
exploration-class space flights
SO FRONTIERS IN SYSTEMS NEUROSCIENCE
LA English
DT Article
DE spaceflight; adaptation; sensorimotor; vestibular; integrative
physiology
ID GALVANIC VESTIBULAR STIMULATION; LONG-DURATION SPACEFLIGHT; DOWN BED
REST; MOTION SICKNESS; PERFORMANCE; BALANCE; ADAPTATION; LOCOMOTION;
RESISTANCE; EXERCISE
AB Research in the area of sensorimotor and neurovestibular function has played an important role in enabling human space flight. This role, however, is changing. One of the key aspects of sensorimotor function relevant to this role will build on its widespread connections with other physiological and psychological systems in the body. The firm knowledge base in this area can provide a strong platform to explore these interactions, which can also provide for the development of effective and efficient countermeasures to the deleterious effects of space flight.
C1 NASA Johnson Space Ctr, NASA Human Res Program, Houston, TX 77058 USA.
RP Shelhamer, M (reprint author), NASA Johnson Space Ctr, NASA Human Res Program, Code 5A2,2101 NASA Parkway, Houston, TX 77058 USA.
EM mark.j.shelhamer@nasa.gov
NR 42
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PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
SN 1662-5137
J9 FRONT SYST NEUROSCI
JI Front. Syst. Neurosci.
PD AUG 11
PY 2015
VL 9
AR 115
DI 10.3389/fnsys.2015.00115
PG 5
WC Neurosciences
SC Neurosciences & Neurology
GA CU9FE
UT WOS:000363848700002
PM 26321927
ER
PT J
AU Gomes, AR
Giacchini, BL
Braga-Ribas, F
Assafin, M
Vieira-Martins, R
Camargo, JIB
Sicardy, B
Timerson, B
George, T
Broughton, J
Blank, T
Benedetti-Rossi, G
Brooks, J
Dantowitz, RF
Dunham, DW
Dunham, JB
Ellington, CK
Emilio, M
Herpich, FR
Jacques, C
Maley, PD
Mehret, L
Mello, AJT
Milone, AC
Pimentel, E
Schoenell, W
Weber, NS
AF Gomes-Junior, A. R.
Giacchini, B. L.
Braga-Ribas, F.
Assafin, M.
Vieira-Martins, R.
Camargo, J. I. B.
Sicardy, B.
Timerson, B.
George, T.
Broughton, J.
Blank, T.
Benedetti-Rossi, G.
Brooks, J.
Dantowitz, R. F.
Dunham, D. W.
Dunham, J. B.
Ellington, C. K.
Emilio, M.
Herpich, F. R.
Jacques, C.
Maley, P. D.
Mehret, L.
Mello, A. J. T.
Milone, A. C.
Pimentel, E.
Schoenell, W.
Weber, N. S.
TI Results of two multichord stellar occultations by dwarf planet (1) Ceres
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE occultations; minor planets, asteroids: individual: (1, Ceres); planets
and satellites: fundamental parameters
ID SHAPE; ALBEDO; RADIUS
AB We report the results of two multichord stellar occultations by the dwarf planet (1) Ceres that were observed from Brazil on 2010 August 17, and from the USA on 2013 October 25. Four positive detections were obtained for the 2010 occultation, and nine for the 2013 occultation. Elliptical models were adjusted to the observed chords to obtain Ceres' size and shape. Two limb-fitting solutions were studied for each event. The first one is a nominal solution with an indeterminate polar aspect angle. The second one was constrained by the pole coordinates as given by Drummond et al. Assuming a Maclaurin spheroid, we determine an equatorial diameter of 972 +/- 6 km and an apparent oblateness of 0.08 +/- 0.03 as our best solution. These results are compared to all available size and shape determinations for Ceres made so far, and shall be confirmed by the NASA's Dawn space mission.
C1 [Gomes-Junior, A. R.; Assafin, M.; Vieira-Martins, R.] Univ Fed Rio de Janeiro, Observ Valongo, Rio de Janeiro, RJ, Brazil.
[Giacchini, B. L.] Ctr Brasileiro Pesquisas Fis, BR-22290180 Rio De Janeiro, Brazil.
[Giacchini, B. L.] REA Brasil, Secao Ocultacoes, BR-31270700 Belo Horizonte, MG, Brazil.
[Giacchini, B. L.; Timerson, B.; George, T.; Blank, T.; Brooks, J.; Dunham, D. W.; Dunham, J. B.; Ellington, C. K.; Maley, P. D.] Int Occultat Timing Assoc, Houston, TX 77219 USA.
[Braga-Ribas, F.; Vieira-Martins, R.; Camargo, J. I. B.; Benedetti-Rossi, G.] Observ Nacl MCTI, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Braga-Ribas, F.] Univ Tecnol Fed Parana, DAFIS, UTFPR, BR-80230901 Curitiba, PR, Brazil.
[Sicardy, B.] Univ Paris Diderot, CNRS UMR 8109, LESIA, Univ Paris 06,Observ Paris, F-92195 Meudon, France.
[Broughton, J.] RASNZ Occultat Sect, Wellington, New Zealand.
[Dantowitz, R. F.; Weber, N. S.] Clay Ctr Observ Dexter Southfield, Brookline, MA 02445 USA.
[Emilio, M.; Mehret, L.] Univ Estadual Ponta Grossa, Observ Astron, DEGEO, BR-84030900 Ponta Grossa, PR, Brazil.
[Herpich, F. R.; Schoenell, W.] Univ Fed Santa Catarina, BR-88040900 Florianopolis, SC, Brazil.
[Jacques, C.; Pimentel, E.] Ctr Estudos Astron Minas Gerais, BR-30140072 Belo Horizonte, MG, Brazil.
[Maley, P. D.] NASA, Johnson Space Ctr Astron Soc, Houston, TX USA.
[Mello, A. J. T.] Univ Tecnol Fed Parana, UTFPR, DAELT, BR-80230901 Curitiba, Parana, Brazil.
[Milone, A. C.] Inst Nacl Pesquisas Espaciais, Div Astrofis, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
RP Gomes, AR (reprint author), Univ Fed Rio de Janeiro, Observ Valongo, Ladeira Pedro Antonio 43, Rio de Janeiro, RJ, Brazil.
EM altair08@astro.ufrj.br; breno@cbpf.br; ribas@on.br
RI Milone, Andre/B-8489-2012; Emilio, Marcelo/C-4118-2011; Schoenell,
William/F-9732-2014; Giacchini, Breno/I-3158-2016; Bueno de Camargo,
Julio Ignacio/C-3145-2013;
OI Emilio, Marcelo/0000-0001-5589-9015; Schoenell,
William/0000-0002-4064-7234; Giacchini, Breno/0000-0002-6449-7189; Bueno
de Camargo, Julio Ignacio/0000-0002-1642-4065; Mello,
Alexandre/0000-0001-9399-0995; Gomes Junior, Altair
Ramos/0000-0002-3362-2127
FU CAPES; PAPDRJ-FAPERJ/CAPES [144997, E-43/2013, E-26/101.375/2014]; CNPq
[473002/2013-2, 482080/2009-4, 312394/2014-4, 308489/2013-6]; FAPERJ
[111.488/2013]; [CNPq-306885/2013]; [Capes/Cofecub-2506/2015];
[Faperj/PAPDRJ-45/2013]
FX ARGJ thanks the financial support of CAPES. BLG thanks CNPq. FBR
acknowledges PAPDRJ-FAPERJ/CAPES E-43/2013 number 144997,
E-26/101.375/2014, and CDFB-CAPES/Brazil. MA acknowledges CNPq grants
473002/2013-2, 482080/2009-4, and 312394/2014-4, and FAPERJ grant
111.488/2013. RVM thanks grants CNPq-306885/2013,
Capes/Cofecub-2506/2015, and Faperj/PAPDRJ-45/2013. JIBC acknowledges
CNPq for a PQ2 fellowship (process number 308489/2013-6). We also
acknowledge Steve Preston for the predictions of the occultations and
the referee Lawrence H. Wasserman (Lowell Observatory) for his
contributions to improve the text.
NR 19
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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 AUG 11
PY 2015
VL 451
IS 3
BP 2295
EP 2302
DI 10.1093/mnras/stv1081
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8CL
UT WOS:000360833700004
ER
PT J
AU Alpaslan, M
Driver, S
Robotham, ASG
Obreschkow, D
Andrae, E
Cluver, M
Kelvin, LS
Lange, R
Owers, M
Taylor, EN
Andrews, SK
Bamford, S
Bland-Hawthorn, J
Brough, S
Brown, MJI
Colless, M
Davies, LJM
Eardley, E
Grootes, MW
Hopkins, AM
Kennedy, R
Liske, J
Lara-Lopez, MA
Lopez-Sanchez, AR
Loveday, J
Madore, BF
Mahajan, S
Meyer, M
Moffett, A
Norberg, P
Penny, S
Pimbblet, KA
Popescu, CC
Seibert, M
Tuffs, R
AF Alpaslan, Mehmet
Driver, Simon
Robotham, Aaron S. G.
Obreschkow, Danail
Andrae, Ellen
Cluver, Michelle
Kelvin, Lee S.
Lange, Rebecca
Owers, Matt
Taylor, Edward N.
Andrews, Stephen K.
Bamford, Steven
Bland-Hawthorn, Joss
Brough, Sarah
Brown, Michael J. I.
Colless, Matthew
Davies, Luke J. M.
Eardley, Elizabeth
Grootes, Meiert W.
Hopkins, Andrew M.
Kennedy, Rebecca
Liske, Jochen
Lara-Lopez, Maritza A.
Lopez-Sanchez, Angel R.
Loveday, Jon
Madore, Barry F.
Mahajan, Smriti
Meyer, Martin
Moffett, Amanda
Norberg, Peder
Penny, Samantha
Pimbblet, Kevin A.
Popescu, Cristina C.
Seibert, Mark
Tuffs, Richard
TI Galaxy And Mass Assembly (GAMA): trends in galaxy colours, morphology,
and stellar populations with large-scale structure, group, and pair
environments
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: clusters: general; galaxies: evolution; galaxies: luminosity
function, mass function; galaxies: stellar content; large-scale
structure of Universe
ID DIGITAL SKY SURVEY; STAR-FORMING GALAXIES; REDSHIFT SURVEY; DARK-MATTER;
METALLICITY RELATION; LUMINOSITY FUNCTION; OPTICAL-PROPERTIES; COSMIC
WEB; CLUSTERS; DEPENDENCE
AB We explore trends in galaxy properties with Mpc-scale structures using catalogues of environment and large-scale structure from the Galaxy And Mass Assembly (GAMA) survey. Existing GAMA catalogues of large-scale structure, group, and pair membership allow us to construct galaxy stellar mass functions for different environmental types. To avoid simply extracting the known underlying correlations between galaxy properties and stellar mass, we create a mass matched sample of galaxies with stellar masses within 9.5 <= logM(*)/h(-2) M-circle dot <= 11 for each environmental population. Using these samples, we show that mass normalized galaxies in different large-scale environments have similar energy outputs, u - r colours, luminosities, and morphologies. Extending our analysis to group and pair environments, we show that galaxies that are not in groups or pairs exhibit similar characteristics to each other regardless of broader environment. For our mass controlled sample, we fail to see a strong dependence of Sersic index or galaxy luminosity on halo mass, but do find that it correlates very strongly with colour. Repeating our analysis for galaxies that have not been mass controlled introduces and amplifies trends in the properties of galaxies in pairs, groups, and large-scale structure, indicating that stellar mass is the most important predictor of the galaxy properties we examine, as opposed to environmental classifications.
C1 [Alpaslan, Mehmet] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Alpaslan, Mehmet; Driver, Simon] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Alpaslan, Mehmet; Driver, Simon; Robotham, Aaron S. G.; Obreschkow, Danail; Lange, Rebecca; Andrews, Stephen K.; Davies, Luke J. M.; Meyer, Martin; Moffett, Amanda] Univ Western Australia, Int Ctr Radio Astron Res, Perth, WA 6009, Australia.
[Andrae, Ellen; Grootes, Meiert W.; Tuffs, Richard] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany.
[Cluver, Michelle] Univ Western Cape, ZA-7535 Cape Town, South Africa.
[Kelvin, Lee S.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Owers, Matt; Lopez-Sanchez, Angel R.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Owers, Matt; Brough, Sarah; Hopkins, Andrew M.; Lopez-Sanchez, Angel R.] Australian Astron Observ, N Ryde, NSW 1670, Australia.
[Taylor, Edward N.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia.
[Bamford, Steven] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Bland-Hawthorn, Joss] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Brown, Michael J. I.; Pimbblet, Kevin A.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Colless, Matthew] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Eardley, Elizabeth] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Liske, Jochen] ESO, D-85748 Garching, Germany.
[Lara-Lopez, Maritza A.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Loveday, Jon] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Madore, Barry F.; Seibert, Mark] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Mahajan, Smriti] IISERM, Manauli 140306, PO, India.
[Norberg, Peder] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Penny, Samantha] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Pimbblet, Kevin A.] Univ Hull, Dept Math & Phys, Kingston Upon Hull HU6 7RX, N Humberside, England.
[Popescu, Cristina C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Popescu, Cristina C.] Romanian Acad, Astron Inst, Bucharest 040557, Romania.
RP Alpaslan, M (reprint author), NASA, Ames Res Ctr, N232, Mountain View, CA 94035 USA.
EM mehmet.alpaslan@nasa.gov
RI Bamford, Steven/E-8702-2010; Brown, Michael/B-1181-2015;
OI Bamford, Steven/0000-0001-7821-7195; Brown, Michael/0000-0002-1207-9137;
Liske, Jochen/0000-0001-7542-2927; Owers, Matt/0000-0002-2879-1663;
Robotham, Aaron/0000-0003-0429-3579; Alpaslan,
Mehmet/0000-0003-0321-1033; Colless, Matthew/0000-0001-9552-8075
FU University of Western Australia; University of St Andrews; STFC (UK);
ARC (Australia); AAO; ESO Telescopes at the La Silla Paranal Observatory
[179.A-2004]
FX The authors acknowledge the reviewer for their detailed and thoughtful
comments on this work. MA is funded by an appointment to the NASA
Postdoctoral Program at Ames Research Centre, administered by Oak Ridge
Associated Universities through a contract with NASA, and acknowledges
past funding from the University of Western Australia and the University
of St Andrews.; GAMA is a joint European-Australasian project based
around a spectroscopic campaign using the Anglo-Australian Telescope.
The GAMA input catalogue is based on data taken from the Sloan Digital
Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging
of the GAMA regions is being obtained by a number of independent survey
programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE,
Herschel-ATLAS, GMRT, and ASKAP providing UV to radio coverage. GAMA is
funded by the STFC (UK), the ARC (Australia), the AAO, and the
participating institutions. The GAMA website is
http://www.gama-survey.org/. The VISTA VIKING data used in this paper
are based on observations made with ESO Telescopes at the La Silla
Paranal Observatory under programme ID 179.A-2004.
NR 94
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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 AUG 11
PY 2015
VL 451
IS 3
BP 3249
EP 3268
DI 10.1093/mnras/stv1176
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CQ8CL
UT WOS:000360833700079
ER
PT J
AU Aartsen, MG
Abraham, K
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Ahrens, M
Altmann, D
Anderson, T
Archinger, M
Arguelles, C
Arlen, TC
Auffenberg, J
Bai, X
Barwick, SW
Baum, V
Bay, R
Beatty, JJ
Tjus, JB
Becker, KH
Beiser, E
BenZvi, S
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Besson, DZ
Binder, G
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Borner, M
Bos, F
Bose, D
Boser, S
Botner, O
Braun, J
Brayeur, L
Bretz, HP
Brown, AM
Buzinsky, N
Casey, J
Casier, M
Cheung, E
Chirkin, D
Christov, A
Christy, B
Clark, K
Classen, L
Coenders, S
Cowen, DF
Silva, AHC
Daughhetee, J
Davis, JC
Day, M
de Andre, JPAM
De Clercq, C
Dembinski, H
De Ridder, S
Desiati, P
de Vries, KD
de Wasseige, G
de With, M
DeYoung, T
Diaz-Velez, JC
Dumm, JP
Dunkman, M
Eagan, R
Eberhardt, B
Ehrhardt, T
Eichmann, B
Euler, S
Evenson, PA
Fadiran, O
Fahey, S
Fazely, AR
Fedynitch, A
Feintzeig, J
Felde, J
Filimonov, K
Finley, C
Fischer-Wasels, T
Flis, S
Fuchs, T
Gaisser, TK
Gaior, R
Gallagher, J
Gerhardt, L
Ghorbani, K
Gier, D
Gladstone, L
Glagla, M
Glusenkamp, T
Goldschmidt, A
Golup, G
Gonzalez, JG
Goodman, JA
Gora, D
Grant, D
Gretskov, P
Groh, JC
Gross, A
Ha, C
Haack, C
Ismail, AH
Hallgren, A
Halzen, F
Hansmann, B
Hanson, K
Hebecker, D
Heereman, D
Helbing, K
Hellauer, R
Hellwig, D
Hickford, S
Hignight, J
Hill, GC
Hoffman, KD
Hoffmann, R
Holzapfel, K
Homeier, A
Hoshina, K
Huang, F
Huber, M
Huelsnitz, W
Hulth, PO
Hultqvist, K
In, S
Ishihara, A
Jacobi, E
Japaridze, GS
Jero, K
Jurkovic, M
Kaminsky, B
Kappes, A
Karg, T
Karle, A
Kauer, M
Keivani, A
Kelley, JL
Kemp, J
Kheirandish, A
Kiryluk, J
Klas, J
Klein, SR
Kohnen, G
Kolanoski, H
Konietz, R
Koob, A
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krings, K
Kroll, G
Kroll, M
Kunnen, J
Kurahashi, N
Kuwabara, T
Labare, M
Lanfranchi, JL
Larson, MJ
Lesiak-Bzdak, M
Leuermann, M
Leuner, J
Lunemann, J
Madsen, J
Maggi, G
Mahn, KBM
Maruyama, R
Mase, K
Matis, HS
Maunu, R
McNally, F
Meagher, K
Medici, M
Meli, A
Menne, T
Merino, G
Meures, T
Miarecki, S
Middell, E
Middlemas, E
Miller, J
Mohrmann, L
Montaruli, T
Morse, R
Nahnhauer, R
Naumann, U
Niederhausen, H
Nowicki, SC
Nygren, DR
Obertacke, A
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
Putz, J
Quinnan, M
Radel, L
Rameez, M
Rawlins, K
Redl, P
Reimann, R
Relich, M
Resconi, E
Rhode, W
Richman, M
Richter, S
Riedel, B
Robertson, S
Rongen, M
Rott, C
Ruhe, T
Ruzybayev, B
Ryckbosch, D
Saba, SM
Sabbatini, L
Sander, HG
Sandrock, A
Sandroos, J
Sarkar, S
Schatto, K
Scheriau, F
Schimp, M
Schmidt, T
Schmitz, M
Schoenen, S
Schoneberg, S
Schonwald, A
Schukraft, A
Schulte, L
Seckel, D
Seunarine, S
Shanidze, R
Smith, MWE
Soldin, D
Spiczak, GM
Spiering, C
Stahlberg, M
Stamatikos, M
Stanev, T
Stanisha, NA
Stasik, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strahler, EA
Strom, R
Strotjohann, NL
Sullivan, GW
Sutherland, M
Taavola, H
Taboada, I
Ter-Antonyan, S
Terliuk, A
Tesic, G
Tilav, S
Toale, PA
Tobin, MN
Tosi, D
Tselengidou, M
Unger, E
Usner, M
Vallecorsa, S
Vandenbroucke, J
van Eijndhoven, N
Vanheule, S
van Santen, J
Veenkamp, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Wallace, A
Wallraff, M
Wandkowsky, N
Weaver, C
Wendt, C
Westerhoff, S
Whelan, BJ
Whitehorn, N
Wichary, C
Wiebe, K
Wiebusch, CH
Wille, L
Williams, DR
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, DL
Xu, XW
Xu, Y
Yanez, JP
Yodh, G
Yoshida, S
Zarzhitsky, P
Zoll, M
AF Aartsen, M. G.
Abraham, K.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Ahrens, M.
Altmann, D.
Anderson, T.
Archinger, M.
Arguelles, C.
Arlen, T. C.
Auffenberg, J.
Bai, X.
Barwick, S. W.
Baum, V.
Bay, R.
Beatty, J. J.
Tjus, J. Becker
Becker, K. -H.
Beiser, E.
BenZvi, S.
Berghaus, P.
Berley, D.
Bernardini, E.
Bernhard, A.
Besson, D. Z.
Binder, G.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Boerner, M.
Bos, F.
Bose, D.
Boeser, S.
Botner, O.
Braun, J.
Brayeur, L.
Bretz, H. -P.
Brown, A. M.
Buzinsky, N.
Casey, J.
Casier, M.
Cheung, E.
Chirkin, D.
Christov, A.
Christy, B.
Clark, K.
Classen, L.
Coenders, S.
Cowen, D. F.
Silva, A. H. Cruz
Daughhetee, J.
Davis, J. C.
Day, M.
de Andre, J. P. A. M.
De Clercq, C.
Dembinski, H.
De Ridder, S.
Desiati, P.
de Vries, K. D.
de Wasseige, G.
de With, M.
DeYoung, T.
Diaz-Velez, J. C.
Dumm, J. P.
Dunkman, M.
Eagan, R.
Eberhardt, B.
Ehrhardt, T.
Eichmann, B.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fahey, S.
Fazely, A. R.
Fedynitch, A.
Feintzeig, J.
Felde, J.
Filimonov, K.
Finley, C.
Fischer-Wasels, T.
Flis, S.
Fuchs, T.
Gaisser, T. K.
Gaior, R.
Gallagher, J.
Gerhardt, L.
Ghorbani, K.
Gier, D.
Gladstone, L.
Glagla, M.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Gonzalez, J. G.
Goodman, J. A.
Gora, D.
Grant, D.
Gretskov, P.
Groh, J. C.
Gross, A.
Ha, C.
Haack, C.
Ismail, A. Haj
Hallgren, A.
Halzen, F.
Hansmann, B.
Hanson, K.
Hebecker, D.
Heereman, D.
Helbing, K.
Hellauer, R.
Hellwig, D.
Hickford, S.
Hignight, J.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Holzapfel, K.
Homeier, A.
Hoshina, K.
Huang, F.
Huber, M.
Huelsnitz, W.
Hulth, P. O.
Hultqvist, K.
In, S.
Ishihara, A.
Jacobi, E.
Japaridze, G. S.
Jero, K.
Jurkovic, M.
Kaminsky, B.
Kappes, A.
Karg, T.
Karle, A.
Kauer, M.
Keivani, A.
Kelley, J. L.
Kemp, J.
Kheirandish, A.
Kiryluk, J.
Klaes, J.
Klein, S. R.
Kohnen, G.
Kolanoski, H.
Konietz, R.
Koob, A.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Krings, K.
Kroll, G.
Kroll, M.
Kunnen, J.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Lanfranchi, J. L.
Larson, M. J.
Lesiak-Bzdak, M.
Leuermann, M.
Leuner, J.
Luenemann, J.
Madsen, J.
Maggi, G.
Mahn, K. B. M.
Maruyama, R.
Mase, K.
Matis, H. S.
Maunu, R.
McNally, F.
Meagher, K.
Medici, M.
Meli, A.
Menne, T.
Merino, G.
Meures, T.
Miarecki, S.
Middell, E.
Middlemas, E.
Miller, J.
Mohrmann, L.
Montaruli, T.
Morse, R.
Nahnhauer, R.
Naumann, U.
Niederhausen, H.
Nowicki, S. C.
Nygren, D. R.
Obertacke, A.
Olivas, A.
Omairat, A.
O'Murchadha, A.
Palczewski, T.
Paul, L.
Pepper, J. A.
de los Heros, C. Perez
Pfendner, C.
Pieloth, D.
Pinat, E.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Puetz, J.
Quinnan, M.
Raedel, L.
Rameez, M.
Rawlins, K.
Redl, P.
Reimann, R.
Relich, M.
Resconi, E.
Rhode, W.
Richman, M.
Richter, S.
Riedel, B.
Robertson, S.
Rongen, M.
Rott, C.
Ruhe, T.
Ruzybayev, B.
Ryckbosch, D.
Saba, S. M.
Sabbatini, L.
Sander, H. -G.
Sandrock, A.
Sandroos, J.
Sarkar, S.
Schatto, K.
Scheriau, F.
Schimp, M.
Schmidt, T.
Schmitz, M.
Schoenen, S.
Schoeneberg, S.
Schoenwald, A.
Schukraft, A.
Schulte, L.
Seckel, D.
Seunarine, S.
Shanidze, R.
Smith, M. W. E.
Soldin, D.
Spiczak, G. M.
Spiering, C.
Stahlberg, M.
Stamatikos, M.
Stanev, T.
Stanisha, N. A.
Stasik, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strahler, E. A.
Strom, R.
Strotjohann, N. L.
Sullivan, G. W.
Sutherland, M.
Taavola, H.
Taboada, I.
Ter-Antonyan, S.
Terliuk, A.
Tesic, G.
Tilav, S.
Toale, P. A.
Tobin, M. N.
Tosi, D.
Tselengidou, M.
Unger, E.
Usner, M.
Vallecorsa, S.
Vandenbroucke, J.
van Eijndhoven, N.
Vanheule, S.
van Santen, J.
Veenkamp, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Wallace, A.
Wallraff, M.
Wandkowsky, N.
Weaver, Ch
Wendt, C.
Westerhoff, S.
Whelan, B. J.
Whitehorn, N.
Wichary, C.
Wiebe, K.
Wiebusch, C. H.
Wille, L.
Williams, D. R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, D. L.
Xu, X. W.
Xu, Y.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
Zoll, M.
CA IceCube Collaboration
TI A COMBINED MAXIMUM-LIKELIHOOD ANALYSIS OF THE HIGH-ENERGY ASTROPHYSICAL
NEUTRINO FLUX MEASURED WITH ICECUBE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astroparticle physics; methods: data analysis; neutrinos
ID GAMMA-RAY SOURCES; COSMIC-RAYS; POINT-LIKE; PERFORMANCE; TELESCOPE;
EMISSION; GALAXIES; SPECTRUM; SEARCHES; SIGNALS
AB Evidence for an extraterrestrial flux of high-energy neutrinos has now been found in multiple searches with the IceCube detector. The first solid evidence was provided by a search for neutrino events with deposited energies greater than or similar to 30 TeV and interaction vertices inside the instrumented volume. Recent analyses suggest that the extraterrestrial flux extends to lower energies and is also visible with throughgoing, nu(mu)-induced tracks from the Northern Hemisphere. Here, we combine the results from six different IceCube searches for astrophysical neutrinos in a maximum-likelihood analysis. The combined event sample features high-statistics samples of shower-like and track-like events. The data are fit in up to three observables: energy, zenith angle, and event topology. Assuming the astrophysical neutrino flux to be isotropic and to consist of equal flavors at Earth, the all-flavor spectrum with neutrino energies between 25 TeV and 2.8 PeV is well described by an unbroken power law with best-fit spectral index -2.50 +/- 0.09 and a flux at 100 TeV of (6.7(-1.2)(+1.1)) x 10(-18) GeV-1 s(-1) sr(-1) cm(-2). Under the same assumptions, an unbroken power law with index -2 is disfavored with a significance of 3.8 sigma (p = 0.0066%) with respect to the best fit. This significance is reduced to 2.1 sigma (p = 1.7%) if instead we compare the best fit to a spectrum with index -2 that has an exponential cut-off at high energies. Allowing the electron-neutrino flux to deviate from the other two flavors, we find a nu(e) fraction of 0.18 +/- 0.11 at Earth. The sole production of electron neutrinos, which would be characteristic of neutron-decay-dominated sources, is rejected with a significance of 3.6 sigma ( p = 0.014%).
C1 [Aartsen, M. G.; Hill, G. C.; Robertson, S.; Wallace, A.; Whelan, B. J.] Univ Adelaide, Dept Phys, Adelaide, SA 5005, Australia.
[Abraham, K.; Bernhard, A.; Coenders, S.; Gross, A.; Holzapfel, K.; Huber, M.; Jurkovic, M.; Krings, K.; Resconi, E.; Veenkamp, J.] Tech Univ Munich, D-85748 Garching, Germany.
[Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Kaminsky, B.; Karg, T.; Kowalski, M.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Spiering, C.; Stasik, A.; Stoessl, A.; Strotjohann, N. L.; Terliuk, A.; Usner, M.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Adams, J.; Brown, A. M.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Aguilar, J. A.; Heereman, D.; Meagher, K.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Bruxelles, Sci Fac CP230, B-1050 Brussels, Belgium.
[Ahlers, M.; Arguelles, C.; Beiser, E.; BenZvi, S.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fadiran, O.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; McNally, F.; Merino, G.; Middlemas, E.; Morse, R.; Richter, S.; Sabbatini, L.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; van Santen, J.; Wandkowsky, N.; Weaver, Ch; Wendt, C.; Westerhoff, S.; Whitehorn, N.; Wille, L.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Ahlers, M.; Arguelles, C.; Beiser, E.; BenZvi, S.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fadiran, O.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; McNally, F.; Merino, G.; Middlemas, E.; Morse, R.; Richter, S.; Sabbatini, L.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; van Santen, J.; Wandkowsky, N.; Weaver, Ch; Wendt, C.; Westerhoff, S.; Whitehorn, N.; Wille, L.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Ahrens, M.; Bohm, C.; Dumm, J. P.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Ahrens, M.; Bohm, C.; Dumm, J. P.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Altmann, D.; Classen, L.; Kappes, A.; Tselengidou, M.] Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Anderson, T.; Arlen, T. C.; Cowen, D. F.; Dunkman, M.; Eagan, R.; Groh, J. C.; Huang, F.; Keivani, A.; Lanfranchi, J. L.; Quinnan, M.; Smith, M. W. E.; Stanisha, N. A.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Archinger, M.; Baum, V.; Boeser, S.; Eberhardt, B.; Ehrhardt, T.; Koepke, L.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Auffenberg, J.; Bissok, M.; Blumenthal, J.; Gier, D.; Glagla, M.; Gretskov, P.; Haack, C.; Hansmann, B.; Hellwig, D.; Kemp, J.; Konietz, R.; Koob, A.; Leuermann, M.; Leuner, J.; Paul, L.; Puetz, J.; Raedel, L.; Reimann, R.; Rongen, M.; Schimp, M.; Schoenen, S.; Schukraft, A.; Stahlberg, M.; Vehring, M.; Wallraff, M.; Wichary, C.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 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.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Tjus, J. Becker; Bos, F.; Eichmann, B.; Fedynitch, A.; Kroll, M.; Saba, S. M.; Schoeneberg, S.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Helbing, K.; Hickford, S.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Omairat, A.; Posselt, J.; Soldin, D.] Berg Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Berley, D.; Blaufuss, E.; Cheung, E.; Christy, B.; Felde, J.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Maunu, R.; Olivas, A.; Redl, P.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 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.
[Boersma, D. J.; Botner, O.; Euler, S.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.; Unger, E.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden.
[Boerner, M.; Fuchs, T.; Menne, T.; Pieloth, D.; Rhode, W.; Ruhe, T.; Sandrock, A.; Scheriau, F.; Schmitz, M.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Bose, D.; In, S.; Rott, C.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
[Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; de Wasseige, G.; Golup, G.; Kunnen, J.; Maggi, G.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Buzinsky, N.; Grant, D.; Kopper, C.; Nowicki, S. C.; Riedel, B.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[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.
[Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[Clark, K.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[de Andre, J. P. A. M.; DeYoung, T.; Hignight, J.; Mahn, K. B. M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[De Ridder, S.; Ismail, A. Haj; Labare, M.; Meli, A.; Ryckbosch, D.; Vanheule, S.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[de With, M.; Hebecker, D.; Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Gaior, R.; Ishihara, A.; Kuwabara, T.; Mase, K.; Relich, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Homeier, A.; Schulte, L.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Kauer, M.; Maruyama, R.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.; Xu, Y.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Koskinen, D. J.; Larson, M. J.; Medici, M.; Sandroos, J.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Kurahashi, N.; Richman, M.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA.
[Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[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.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Mohrmann, L (reprint author), DESY, D-15735 Zeuthen, Germany.
EM lars.mohrmann@desy.de
RI Tjus, Julia/G-8145-2012; Sarkar, Subir/G-5978-2011; Beatty,
James/D-9310-2011; Maruyama, Reina/A-1064-2013; Wiebusch,
Christopher/G-6490-2012; Koskinen, David/G-3236-2014;
OI Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952;
Maruyama, Reina/0000-0003-2794-512X; Wiebusch,
Christopher/0000-0002-6418-3008; Koskinen, David/0000-0002-0514-5917;
Maunu, Ryan/0000-0002-5755-3437; 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) at the
University of Wisconsin-Madison; Open Science Grid (OSG); U.S.
Department of Energy; National Energy Research Scientific Computing
Center; Louisiana Optical Network Initiative (LONI); Natural Sciences
and Engineering Research Council of Canada; WestGrid; Compute/Calcul
Canada; Swedish Research Council, Sweden; Swedish Polar Research
Secretariat, Sweden; Swedish National Infrastructure for Computing
(SNIC), Sweden; Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF), Germany; Deutsche
Forschungsgemeinschaft (DFG), Germany; Helmholtz Alliance for
Astroparticle Physics (HAP), Germany; 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).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2015
VL 809
IS 1
AR 98
DI 10.1088/0004-637X/809/1/98
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500098
ER
PT J
AU Allred, JC
Kowalski, AF
Carlsson, M
AF Allred, Joel C.
Kowalski, Adam F.
Carlsson, Mats
TI A UNIFIED COMPUTATIONAL MODEL FOR SOLAR AND STELLAR FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: numerical; radiative transfer; stars: flare; Sun: atmosphere;
Sun: flares
ID RADIATIVE HYDRODYNAMIC MODELS; X-RAY-SPECTRA; ELECTRON-BEAMS; HYDROGEN
LINES; RETURN-CURRENT; AD LEONIS; ULTRAVIOLET EMISSION; ATOMIC DATABASE;
MAGNETIC-FIELD; CROSS-SECTIONS
AB We present a unified computational framework that can be used to describe impulsive flares on the Sun and on dMe stars. The models assume that the flare impulsive phase is caused by a beam of charged particles that is accelerated in the corona and propagates downward depositing energy and momentum along the way. This rapidly heats the lower stellar atmosphere causing it to explosively expand and dramatically brighten. Our models consist of flux tubes that extend from the sub-photosphere into the corona. We simulate how flare-accelerated charged particles propagate down one-dimensional flux tubes and heat the stellar atmosphere using the Fokker-Planck kinetic theory. Detailed radiative transfer is included so that model predictions can be directly compared with observations. The flux of flare-accelerated particles drives return currents which additionally heat the stellar atmosphere. These effects are also included in our models. We examine the impact of the flare-accelerated particle beams on model solar and dMe stellar atmospheres and perform parameter studies varying the injected particle energy spectra. We find the atmospheric response is strongly dependent on the accelerated particle cutoff energy and spectral index.
C1 [Allred, Joel C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kowalski, Adam F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Carlsson, Mats] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway.
RP Allred, JC (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
EM joel.c.allred@nasa.gov
OI Carlsson, Mats/0000-0001-9218-3139
FU NASA Heliophysics Supporting Research and Technology; NASA Living With a
Star programs; NASA Postdoctoral Program at the Goddard Space Flight
Center; UMCP GPHI Task 132; European Research Council under the European
Union's Seventh Framework Programme (FP7)/ERC grant [291058]; Research
Council of Norway
FX This work has been supported by grants through the NASA Heliophysics
Supporting Research and Technology and the NASA Living With a Star
programs. This research was aided by many useful discussions with the
participants of the Chromospheric Flares meeting held at the
International Space Science Institute (ISSI) in Bern, Switzerland.
A.F.K. acknowledges the support of the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by Oak Ridge Associated
Universities through a contract with NASA, and from support through UMCP
GPHI Task 132. 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 nr
291058 and by the Research Council of Norway through the grant "Solar
Atmospheric Modelling" and through grants of computing time from the
Programme for Supercomputing. We thank G. Holman for helpful discussions
about return current heating.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2015
VL 809
IS 1
AR 104
DI 10.1088/0004-637X/809/1/104
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500104
ER
PT J
AU Barclay, T
Quintana, EV
Adams, FC
Ciardi, DR
Huber, D
Foreman-Mackey, D
Montet, BT
Caldwell, D
AF Barclay, Thomas
Quintana, Elisa V.
Adams, Fred C.
Ciardi, David R.
Huber, Daniel
Foreman-Mackey, Daniel
Montet, Benjamin T.
Caldwell, Douglas
TI THE FIVE PLANETS IN THE KEPLER-296 BINARY SYSTEM ALL ORBIT THE PRIMARY:
A STATISTICAL AND ANALYTICAL ANALYSIS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; methods: data analysis; methods: statistical;
planetary systems; stars: individual (Kepler-296, KIC 11497958,
KOI-1422); techniques: photometric
ID POTENTIAL TRANSIT SIGNALS; CANDIDATE HOST STARS; EARTH-SIZED PLANET;
SOLAR-TYPE STARS; HABITABLE ZONE; BAYESIAN-INFERENCE; MISSION DATA;
DENSE CORES; DARK CLOUDS; M DWARFS
AB Kepler-296 is a binary star system with two M-dwarf components separated by 0 ''.2. Five transiting planets have been confirmed to be associated with the Kepler-296 system; given the evidence to date, however, the planets could in principle orbit either star. This ambiguity has made it difficult to constrain both the orbital and physical properties of the planets. Using both statistical and analytical arguments, this paper shows that all five planets are highly likely to orbit the primary star in this system. We performed a Markov-Chain Monte Carlo simulation using a five transiting planet model, leaving the stellar density and dilution with uniform priors. Using importance sampling, we compared the model probabilities under the priors of the planets orbiting either the brighter or the fainter component of the binary. A model where the planets orbit the brighter component, Kepler-296A, is strongly preferred by the data. Combined with our assertion that all five planets orbit the same star, the two outer planets in the system, Kepler-296 Ae and Kepler-296 Af, have radii of 1.53 +/- 0.26 and 1.80 +/- 0.31 R-circle plus, respectively, and receive incident stellar fluxes of 1.40 +/- 0.23 and 0.62 +/- 0.10 times the incident flux the Earth receives from the Sun. This level of irradiation places both planets within or close to the circumstellar habitable zone of their parent star.
C1 [Barclay, Thomas; Quintana, Elisa V.; Caldwell, Douglas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
[Adams, Fred C.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Huber, Daniel; Caldwell, Douglas] SETI Inst, Mountain View, CA 94043 USA.
[Huber, Daniel] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Foreman-Mackey, Daniel] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Montet, Benjamin T.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Montet, Benjamin T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Barclay, T (reprint author), NASA, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA.
OI Montet, Benjamin/0000-0001-7516-8308; Ciardi, David/0000-0002-5741-3047
FU NASA Science Mission Directorate; Association of Universities for
Research in Astronomy, Inc., under NASA [NAS5-26555]; NASA Office of
Space Science [NNX09AF08G]; NASA Keck PI Data Award; W. M. Keck
Foundation; NASA Senior Fellowship at the Ames Research Center; National
Science Foundation Graduate Research Fellowship [DGE1144469]; Australian
Research Council [DE140101364]; National Aeronautics and Space
Administration [NNX14AB92G]
FX This paper includes data collected by the Kepler mission. Funding for
the Kepler mission is provided by the NASA Science Mission Directorate.
We would like to express our gratitude to all those who have worked on
the Kepler pipeline over the many years of the Kepler mission. Some
Kepler data presented in this paper were obtained from the Mikulski
Archive for Space Telescopes (MAST) at the Space Telescope Science
Institute (STScI). 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 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 made use of APLpy, an open-source
plotting package for Python hosted at http://aplpy.github.com. This work
was supported by a NASA Keck PI Data Award, administered by the NASA
Exoplanet Science Institute. Some of the 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. The authors
wish to recognize and acknowledge the very significant cultural role and
reverence that the summit of Maunakea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. E.V.Q. is
supported by a NASA Senior Fellowship at the Ames Research Center,
administered by Oak Ridge Associated Universities through a contract
with NASA. B.T.M. is supported by the National Science Foundation
Graduate Research Fellowship under Grant No. DGE1144469. D.H.
acknowledges support by the Australian Research Council's Discovery
Projects funding scheme (project number DE140101364) and support by the
National Aeronautics and Space Administration under Grant NNX14AB92G
issued through the Kepler Participating Scientist Program.
NR 62
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2015
VL 809
IS 1
DI 10.1088/0004-637X/809/1/7
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500007
ER
PT J
AU Bottom, M
Kuhn, J
Mennesson, B
Mawet, D
Shelton, JC
Wallace, JK
Serabyn, E
AF Bottom, Michael
Kuhn, Jonas
Mennesson, Bertrand
Mawet, Dimitri
Shelton, Jean C.
Wallace, J. Kent
Serabyn, Eugene
TI RESOLVING THE DELTA ANDROMEDAE SPECTROSCOPIC BINARY WITH DIRECT IMAGING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: spectroscopic; instrumentation: adaptive optics;
instrumentation: high angular resolution; stars: imaging
ID ADAPTIVE OPTICS; HIPPARCOS; ASTROMETRY
AB We present a direct image of the innermost companion to the red giant delta Andromedae using the Stellar Double Coronagraph at the Palomar Observatory. We use a Markov Chain Monte Carlo based algorithm to simultaneously reduce the data and perform astrometry and photometry of the companion. We determine that the companion is most likely a main sequence K-type star and is certainly not the previously hypothesized white dwarf.
C1 [Bottom, Michael; Mawet, Dimitri] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Kuhn, Jonas; Mennesson, Bertrand; Shelton, Jean C.; Wallace, J. Kent; Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kuhn, Jonas] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
RP Bottom, M (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, MC 249-17, Pasadena, CA 91125 USA.
EM mbottom@caltech.edu
RI Kuhn, Jonas/H-2338-2011
OI Kuhn, Jonas/0000-0002-6344-4835
FU NASA Space Technology Research Fellowship [NNX13AN42H]
FX We are pleased to acknowledge the Palomar Observatory staff for their
excellent support, particularly Steve Kunsman. We greatly benefited from
the expert assistance of Rick Burruss (JPL) with the adaptive optics
system. We thank the referee for a useful review, particularly for
pointing out some discrepancies in our analysis and previous work, which
improved the paper. Part of this work was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration (NASA).
M.B. is supported by a NASA Space Technology Research Fellowship, grant
NNX13AN42H.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2015
VL 809
IS 1
AR 11
DI 10.1088/0004-637X/809/1/11
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500011
ER
PT J
AU Burke, CJ
Christiansen, JL
Mullally, F
Seader, S
Huber, D
Rowe, JF
Coughlin, JL
Thompson, SE
Catanzarite, J
Clarke, BD
Morton, TD
Caldwell, DA
Bryson, ST
Haas, MR
Batalha, NM
Jenkins, JM
Tenenbaum, P
Twicken, JD
Li, J
Quintana, E
Barclay, T
Henze, CE
Borucki, WJ
Howell, SB
Still, M
AF Burke, Christopher J.
Christiansen, Jessie L.
Mullally, F.
Seader, Shawn
Huber, Daniel
Rowe, Jason F.
Coughlin, Jeffrey L.
Thompson, Susan E.
Catanzarite, Joseph
Clarke, Bruce D.
Morton, Timothy D.
Caldwell, Douglas A.
Bryson, Stephen T.
Haas, Michael R.
Batalha, Natalie M.
Jenkins, Jon M.
Tenenbaum, Peter
Twicken, Joseph D.
Li, Jie
Quintana, Elisa
Barclay, Thomas
Henze, Christopher E.
Borucki, William J.
Howell, Steve B.
Still, Martin
TI TERRESTRIAL PLANET OCCURRENCE RATES FOR THE KEPLER GK DWARF SAMPLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; eclipses; methods: statistical; planetary systems; space
vehicles; surveys Supporting material: machine-readable tables
ID TRANSITING EXTRASOLAR PLANETS; SUN-LIKE STARS; CANDIDATE HOST STARS;
MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; R-CIRCLE-PLUS; HABITABLE-ZONE;
LIGHT CURVES; MISSION DATA; GALACTIC BULGE
AB We measure planet occurrence rates using the planet candidates discovered by the Q1-Q16 Kepler pipeline search. This study examines planet occurrence rates for the Kepler GK dwarf target sample for planet radii, 0.75 <= R-p <= 2.5 R-circle plus, and orbital periods, 50 <= P-orb <= 300 days, with an emphasis on a thorough exploration and identification of the most important sources of systematic uncertainties. Integrating over this parameter space, we measure an occurrence rate of F-0 = 0.77 planets per star, with an allowed range of 0.3 <= F-0 <= 1.9. The allowed range takes into account both statistical and systematic uncertainties, and values of F0 beyond the allowed range are significantly in disagreement with our analysis. We generally find higher planet occurrence rates and a steeper increase in planet occurrence rates toward small planets than previous studies of the Kepler GK dwarf sample. Through extrapolation, we find that the one year orbital period terrestrial planet occurrence rate zeta(1.0) = 0.1, with an allowed range of 0.01 <= zeta(1.0) <= 2, where zeta(1.0) is defined as the number of planets per star within 20% of the R-p and P-orb of Earth. For G dwarf hosts, the zeta(1.0) parameter space is a subset of the larger eta(circle plus) parameter space, thus zeta(1.0) places a lower limit on eta(circle plus) for G dwarf hosts. From our analysis, we identify the leading sources of systematics impacting Kepler occurrence rate determinations as reliability of the planet candidate sample, planet radii, pipeline completeness, and stellar parameters.
C1 [Burke, Christopher J.; Mullally, F.; Seader, Shawn; Rowe, Jason F.; Coughlin, Jeffrey L.; Thompson, Susan E.; Catanzarite, Joseph; Clarke, Bruce D.; Caldwell, Douglas A.; Tenenbaum, Peter; Twicken, Joseph D.; Li, Jie; Quintana, Elisa] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Christiansen, Jessie L.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA.
[Huber, Daniel] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Morton, Timothy D.] Princeton Univ, Dept Astrophys, Princeton, NJ 08544 USA.
[Bryson, Stephen T.; Haas, Michael R.; Batalha, Natalie M.; Jenkins, Jon M.; Henze, Christopher E.; Borucki, William J.; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, BAERI, Moffett Field, CA 94035 USA.
RP Burke, CJ (reprint author), NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
EM christopher.j.burke@nasa.gov
FU NASA's Science Mission Directorate; Australian Research Council
[DE140101364]; National Aeronautics and Space Administration
[NNX14AB92G]
FX We thank the referee for insightful suggestions which improved the
manuscript. Funding for this Discovery mission is provided by NASA's
Science Mission Directorate. 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. D.H.
acknowledges support by the Australian Research Council's Discovery
Projects funding scheme (project number DE140101364) and support by the
National Aeronautics and Space Administration under grant NNX14AB92G
issued through the Kepler Participating Scientist Program.
NR 122
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SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2015
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IS 1
DI 10.1088/0004-637X/809/1/8
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500008
ER
PT J
AU Ciardi, DR
Van Eyken, JC
Barnes, JW
Beichman, CA
Carey, SJ
Crockett, CJ
Eastman, J
Johns-Krull, CM
Howell, SB
Kane, SR
Mclane, JN
Plavchan, P
Prato, L
Stauffer, J
Van Belle, GT
Von Braun, K
AF Ciardi, David R.
Van Eyken, Julian C.
Barnes, Jason W.
Beichman, Charles A.
Carey, Sean J.
Crockett, Christopher J.
Eastman, Jason
Johns-Krull, Christopher M.
Howell, Steve B.
Kane, Stephen R.
Mclane, Jacob N. .
Plavchan, Peter
Prato, L.
Stauffer, John
Van Belle, Gerard T.
Von Braun, Kaspar
TI FOLLOW-UP OBSERVATIONS OF PTFO 8-8695: A 3 MYR OLD T TAURI STAR HOSTING
A JUPITER-MASS PLANETARY CANDIDATE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (PTFO 8-8695, 2MASS
J05250755+0134243, CVSO 30); stars: pre-main sequence
ID SPIN-ORBIT MISALIGNMENT; RADIAL-VELOCITY; ORION PROJECT; LIGHT-CURVE;
TRANSIT; VARIABILITY; SYSTEM; SEARCH; BINARY; OCCULTATIONS
AB We present Spitzer 4.5 mu m light curve observations, Keck NIRSPEC radial velocity observations, and LCOGT optical light curve observations of PTFO 8-8695, which may host a Jupiter-sized planet in a very short orbital period (0.45 days). Previous work by van Eyken et al. and Barnes et al. predicts that the stellar rotation axis and the planetary orbital plane should precess with a period of 300-600 days. As a consequence, the observed transits should change shape and depth, disappear, and reappear with the precession. Our observations indicate the long-term presence of the transit events (> 3 years), and that the transits indeed do change depth, disappear and reappear. The Spitzer observations and the NIRSPEC radial velocity observations (with contemporaneous LCOGT optical light curve data) are consistent with the predicted transit times and depths for the M-k = 0.34 M-circle dot precession model and demonstrate the disappearance of the transits. An LCOGT optical light curve shows that the transits do reappear approximately 1 year later. The observed transits occur at the times predicted by a straight-forward propagation of the transit ephemeris. The precession model correctly predicts the depth and time of the Spitzer transit and the lack of a transit at the time of the NIRSPEC radial velocity observations. However, the precession model predicts the return of the transits approximately 1 month later than observed by LCOGT. Overall, the data are suggestive that the planetary interpretation of the observed transit events may indeed be correct, but the precession model and data are currently insufficient to confirm firmly the planetary status of PTFO 8-8695b.
C1 [Ciardi, David R.; Van Eyken, Julian C.; Beichman, Charles A.] NASA Exoplanet Sci Inst Caltech, Pasadena, CA 91125 USA.
[Van Eyken, Julian C.] Univ Calif Santa Barbara, LCOGT, Santa Barbara, CA 93106 USA.
[Barnes, Jason W.; Eastman, Jason] Cumbres Observ Global Telescope Network, Goleta, CA USA.
[Barnes, Jason W.] Univ Idaho, Moscow, ID 83843 USA.
[Carey, Sean J.; Stauffer, John] Spitzer Sci Ctr Caltech, Pasadena, CA USA.
[Crockett, Christopher J.] Sci News, Washington, DC 20036 USA.
[Eastman, Jason] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Johns-Krull, Christopher M.] Rice Univ, Houston, TX USA.
[Howell, Steve B.] NASA Ames Res Ctr, Mountain View, CA USA.
[Kane, Stephen R.] San Francisco State Univ, San Francisco, CA 94132 USA.
[Mclane, Jacob N. .; Prato, L.; Van Belle, Gerard T.; Von Braun, Kaspar] Lowell Observ, Flagstaff, AZ 86001 USA.
[Plavchan, Peter] Missouri State Univ, Springfield, MO USA.
RP Ciardi, DR (reprint author), NASA Exoplanet Sci Inst Caltech, Pasadena, CA 91125 USA.
EM ciardi@ipac.caltech.edu
RI Barnes, Jason/B-1284-2009;
OI Barnes, Jason/0000-0002-7755-3530; Eastman, Jason/0000-0003-3773-5142;
Ciardi, David/0000-0002-5741-3047
FU W. M. Keck Foundation; Las Cumbres Observatory Global Telescope Network;
NASA; National Aeronautics and Space Administration under the Exoplanet
Exploration Program; National Aeronautics and Space Administration
FX D.R.C. would like to dedicate this paper to his dad Robert A. Ciardi
(1940-2013). Robert Ciardi had a passion for learning and knowledge and,
in particular, for science. While not able to pursue a career in science
for himself, he never stopped thinking and growing, and through his love
and encouragement, D.R.C. was able to pursue his own love of exploration
and science. In many ways, Robert Ciardi was more excited about this
discovery than the authors on this paper. He will be greatly missed.
Thank you, Dad. 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 the National Aeronautics and Space Administration. The
Observatory was made possible by the generous financial support of the
W. M. Keck Foundation. The authors wish to recognize and acknowledge the
significant cultural role and reverence that the summit of Mauna Kea has
always had within the indigenous Hawaiian community. We are most
fortunate to have the opportunity to conduct observations from this
mountain. This research has made use of the LCOGT Archive, which is
operated by the California Institute of Technology, under contract with
the Las Cumbres Observatory Global Telescope Network. This work is
based, in part, on observations made with the Spitzer Space Telescope,
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology under a contract with NASA. 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.
Portions of this work were performed at the California Institute of
Technology under contract with the National Aeronautics and Space
Administration.
NR 58
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2015
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IS 1
AR 42
DI 10.1088/0004-637X/809/1/42
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500042
ER
PT J
AU Errard, J
Ade, PAR
Akiba, Y
Arnold, K
Atlas, M
Baccigalupi, C
Barron, D
Boettger, D
Borrill, J
Chapman, S
Chinone, Y
Cukierman, A
Delabrouille, J
Dobbs, M
Ducout, A
Elleflot, T
Fabbian, G
Feng, C
Feeney, S
Gilbert, A
Goeckner-Wald, N
Halverson, NW
Hasegawa, M
Hattori, K
Hazumi, M
Hill, C
Holzapfel, WL
Hori, Y
Inoue, Y
Jaehnig, GC
Jaffe, AH
Jeong, O
Katayama, N
Kaufman, J
Keating, B
Kermish, Z
Keskitalo, R
Kisner, T
Le Jeune, M
Lee, AT
Leitch, EM
Leon, D
Linder, E
Matsuda, F
Matsumura, T
Miller, NJ
Myers, MJ
Navaroli, M
Nishino, H
Okamura, T
Paar, H
Peloton, J
Poletti, D
Puglisi, G
Rebeiz, G
Reichardt, CL
Richards, PL
Ross, C
Rotermund, KM
Schenck, DE
Sherwin, BD
Siritanasak, P
Smecher, G
Stebor, N
Steinbach, B
Stompor, R
Suzuki, A
Tajima, O
Takakura, S
Tikhomirov, A
Tomaru, T
Whitehorn, N
Wilson, B
Yadav, A
Zahn, O
AF Errard, J.
Ade, P. A. R.
Akiba, Y.
Arnold, K.
Atlas, M.
Baccigalupi, C.
Barron, D.
Boettger, D.
Borrill, J.
Chapman, S.
Chinone, Y.
Cukierman, A.
Delabrouille, J.
Dobbs, M.
Ducout, A.
Elleflot, T.
Fabbian, G.
Feng, C.
Feeney, S.
Gilbert, A.
Goeckner-Wald, N.
Halverson, N. W.
Hasegawa, M.
Hattori, K.
Hazumi, M.
Hill, C.
Holzapfel, W. L.
Hori, Y.
Inoue, Y.
Jaehnig, G. C.
Jaffe, A. H.
Jeong, O.
Katayama, N.
Kaufman, J.
Keating, B.
Kermish, Z.
Keskitalo, R.
Kisner, T.
Le Jeune, M.
Lee, A. T.
Leitch, E. M.
Leon, D.
Linder, E.
Matsuda, F.
Matsumura, T.
Miller, N. J.
Myers, M. J.
Navaroli, M.
Nishino, H.
Okamura, T.
Paar, H.
Peloton, J.
Poletti, D.
Puglisi, G.
Rebeiz, G.
Reichardt, C. L.
Richards, P. L.
Ross, C.
Rotermund, K. M.
Schenck, D. E.
Sherwin, B. D.
Siritanasak, P.
Smecher, G.
Stebor, N.
Steinbach, B.
Stompor, R.
Suzuki, A.
Tajima, O.
Takakura, S.
Tikhomirov, A.
Tomaru, T.
Whitehorn, N.
Wilson, B.
Yadav, A.
Zahn, O.
TI MODELING ATMOSPHERIC EMISSION FOR CMB GROUND-BASED OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atmospheric effects; methods: data analysis; methods: observational
ID MICROWAVE BACKGROUND EXPERIMENTS; COMPONENT SEPARATION; FLUCTUATIONS;
POLARIZATION; TURBULENCE; SITES; NOISE
AB Atmosphere is one of the most important noise sources for ground-based cosmic microwave background (CMB) experiments. By increasing optical loading on the detectors, it amplifies their effective noise, while its fluctuations introduce spatial and temporal correlations between detected signals. We present a physically motivated 3D-model of the atmosphere total intensity emission in the millimeter and sub-millimeter wavelengths. We derive a new analytical estimate for the correlation between detectors time-ordered data as a function of the instrument and survey design, as well as several atmospheric parameters such as wind, relative humidity, temperature and turbulence characteristics. Using an original numerical computation, we examine the effect of each physical parameter on the correlations in the time series of a given experiment. We then use a parametric-likelihood approach to validate the modeling and estimate atmosphere parameters from the POLARBEAR-I project first season data set. We derive a new 1.0% upper limit on the linear polarization fraction of atmospheric emission. We also compare our results to previous studies and weather station measurements. The proposed model can be used for realistic simulations of future ground-based CMB observations.
C1 [Errard, J.; Borrill, J.; Kisner, T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Errard, J.; Borrill, J.; Keskitalo, R.; Kisner, T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Ade, P. A. R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3XQ, S Glam, Wales.
[Akiba, Y.; Chinone, Y.; Hasegawa, M.; Hattori, K.; Hazumi, M.; Inoue, Y.; Okamura, T.; Tajima, O.; Takakura, S.; Tomaru, T.] High Energy Accelerator Org KEK, Tsukuba, Ibaraki 3050801, Japan.
[Arnold, K.; Atlas, M.; Barron, D.; Elleflot, T.; Kaufman, J.; Keating, B.; Leon, D.; Matsuda, F.; Navaroli, M.; Paar, H.; Siritanasak, P.; Stebor, N.; Wilson, B.; Yadav, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Baccigalupi, C.; Fabbian, G.; Puglisi, G.] Int Sch Adv Studies SISSA, I-34014 Trieste, Italy.
[Boettger, D.] Pontificia Univ Catolica Chile, Dept Astron, Santiago, Chile.
[Chapman, S.; Ross, C.; Rotermund, K. M.; Tikhomirov, A.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada.
[Chinone, Y.; Cukierman, A.; Goeckner-Wald, N.; Hill, C.; Holzapfel, W. L.; Hori, Y.; Jeong, O.; Lee, A. T.; Myers, M. J.; Richards, P. L.; Sherwin, B. D.; Steinbach, B.; Suzuki, A.; Whitehorn, N.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Delabrouille, J.; Le Jeune, M.; Peloton, J.; Poletti, D.; Stompor, R.] Univ Paris Diderot, Sorbonne Paris Cite, AstroParticule & Cosmol, CNRS,IN2P3,CEA,Irfu,Obs Paris, Paris, France.
[Dobbs, M.; Gilbert, A.; Smecher, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 0G4, Canada.
[Ducout, A.; Feeney, S.; Jaffe, A. H.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England.
[Feng, C.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA.
[Halverson, N. W.; Jaehnig, G. C.; Schenck, D. E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[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.
[Hasegawa, M.; Hazumi, M.] Grad Univ Adv Studies, Miura Dist, Kanagawa 2400115, Japan.
[Hazumi, M.; Katayama, N.; Nishino, H.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan.
[Kermish, Z.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Lee, A. T.; Linder, E.; Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[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.
[Matsumura, T.] JAXA, Chofu, Tokyo, Japan.
[Miller, N. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Rebeiz, G.] Univ Calif San Diego, Dept Elect & Comp Engn, La Jolla, CA 92093 USA.
[Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia.
[Sherwin, B. D.] Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA.
[Takakura, S.] Osaka Univ, Toyonaka, Osaka 5600043, Japan.
RP Errard, J (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
OI Fabbian, Giulio/0000-0002-3255-4695; Reichardt,
Christian/0000-0003-2226-9169
FU Department of Energy [DE-AC02-05CH11231]; National Science Foundation
[AST-0618398, AST-1212230]; Comision Nacional de Investigacion
Cientifica y Tecnologica de Chile (CONICYT)
FX Calculations were performed on the National Energy Research Scientific
Computing (NERSC), supported by the Department of Energy under Contract
No. DE-AC02-05CH11231. The POLARBEAR project is funded by the National
Science Foundation under grants AST-0618398 and AST-1212230. The James
Ax Observatory operates in the Parque Astronomico Atacama in Northern
Chile under the auspices of the Comision Nacional de Investigacion
Cientifica y Tecnologica de Chile (CONICYT). Finally, we would like to
acknowledge the tremendous contributions by Huan Tran to the POLARBEAR
instrument and who has been at the initiation of this particular project
on atmosphere characterization.
NR 39
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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 AUG 10
PY 2015
VL 809
IS 1
AR 63
DI 10.1088/0004-637X/809/1/63
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500063
ER
PT J
AU Gopalswamy, N
Yashiro, S
Akiyama, S
AF Gopalswamy, N.
Yashiro, S.
Akiyama, S.
TI KINEMATIC AND ENERGETIC PROPERTIES OF THE 2012 MARCH 12 POLAR CORONAL
MASS EJECTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: coronal mass ejections (CMEs); Sun: filaments, prominences; Sun:
flares; Sun: magnetic fields
ID MAGNETIC-FLUX; SOLAR-FLARES; NOBEYAMA RADIOHELIOGRAPH; MICROWAVE
OBSERVATIONS; PROMINENCE ERUPTIONS; FILAMENT ERUPTIONS; PARTICLE EVENTS;
ACTIVE REGIONS; SUN; INITIATION
AB We report on the energetics of the 2012 March 12 polar coronal mass ejection (CME) originating from a southern latitude of similar to 60 degrees. The polar CME is similar to low-latitude (LL) CMEs in almost all respects: three-part morphology; post-eruption arcade (PEA), CME, and filament kinematics; CME mass and kinetic energy; and the relative thermal energy content of the PEA. From polarized brightness images, we estimate the CME mass, which is close to the average mass of LL CMEs. The CME kinetic energy (3.3 x 10(30) erg) is also typical of the general population of CMEs. From photospheric magnetograms, we estimate the free energy (1.8 x 10(31) erg) in the polar crown source region, which we find is sufficient to power the CME and the PEA. About 19% of the free energy went into the CME kinetic energy. We compute the thermal energy content of the PEA (2.3 x 10(29) erg) and find it to be a small fraction (6.8%) of the CME kinetic energy. This fraction is remarkably similar to that in active region CMEs associated with major flares. We also show that the 2012 March 12 is one among scores of polar CMEs observed during the maximum phase of cycle 24. The cycle 24 polar crown prominence eruptions have the same rate of association with CMEs as those from LLs. This investigation supports the view that all CMEs are magnetically propelled from closed field regions, irrespective of their location on the Sun (polar crown filament regions, quiescent filament regions, or active regions).
C1 [Gopalswamy, N.; Yashiro, S.; Akiyama, S.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Yashiro, S.; Akiyama, S.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
EM nat.gopalswamy@nasa.gov
FU NASA
FX This research benefited from NASA's open data policy in making the SOHO,
STEREO, and SDO data available on line. This work was supported by
NASA's LWS TR&T program.
NR 59
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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 AUG 10
PY 2015
VL 809
IS 1
AR 106
DI 10.1088/0004-637X/809/1/106
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500106
ER
PT J
AU Grav, T
Bauer, JM
Mainzer, AK
Masiero, JR
Nugent, CR
Cutri, RM
Sonnett, S
Kramer, E
AF Grav, T.
Bauer, J. M.
Mainzer, A. K.
Masiero, J. R.
Nugent, C. R.
Cutri, R. M.
Sonnett, S.
Kramer, E.
TI NEOWISE: OBSERVATIONS OF THE IRREGULAR SATELLITES OF JUPITER AND SATURN
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: planetary systems; planets and satellites: detection; planets
and satellites: fundamental parameters; surveys
ID INFRARED-SURVEY-EXPLORER; OUTER JOVIAN-SATELLITES; MAIN-BELT ASTEROIDS;
4 TROJAN ASTEROIDS; WISE/NEOWISE OBSERVATIONS; SOLAR-SYSTEM; PHOTOMETRIC
PROPERTIES; GAS-DRAG; PHOEBE; CAPTURE
AB We present thermal model fits for 11 Jovian and 3 Saturnian irregular satellites based on measurements from the WISE/NEOWISE data set. Our fits confirm spacecraft-measured diameters for the objects with in situ observations (Himalia and Phoebe) and provide diameters and albedo for 12 previously unmeasured objects, 10 Jovian and 2 Saturnian irregular satellites. The best-fit thermal model beaming parameters are comparable to what is observed for other small bodies in the outer solar system, while the visible, W1, and W2 albedos trace the taxonomic classifications previously established in the literature. Reflectance properties for the irregular satellites measured are similar to the Jovian Trojan and Hilda Populations, implying common origins.
C1 [Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Bauer, J. M.; Mainzer, A. K.; Masiero, J. R.; Sonnett, S.; Kramer, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, J. M.; Nugent, C. R.; Cutri, R. M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
RP Grav, T (reprint author), Planetary Sci Inst, Tucson, AZ 85719 USA.
EM tgrav@psi.edu
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 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. 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 gratefully acknowledge
the extraordinary services specific to NEOWISE that were 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 Jet Propulsion Laboratory/California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. We also thank Fredrick Pilcher, of Organ Mesa
Observatory in Las Cruces, New Mexico, for providing us with the light
curve data of JVI Himalia from his paper (Pilcher et al. 2012).
NR 67
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U1 0
U2 2
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2015
VL 809
IS 1
DI 10.1088/0004-637X/809/1/3
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500003
ER
PT J
AU Henry, A
Scarlata, C
Martin, CL
Erb, D
AF Henry, Alaina
Scarlata, Claudia
Martin, Crystal L.
Erb, Dawn
TI Ly alpha EMISSION FROM GREEN PEAS: THE ROLE OF CIRCUMGALACTIC GAS
DENSITY, COVERING, AND KINEMATICS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: formation
ID STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; DIGITAL-SKY-SURVEY;
SIMILAR-TO 7; GREATER-THAN 7; KECK SPECTROSCOPY; LUMINOSITY FUNCTION;
OPTICAL DEPTH; CHEMICAL-COMPOSITION; ULTRAVIOLET-SPECTRA
AB We report Hubble Space Telescope/Cosmic Origins Spectrograph observations of the Ly alpha emission and interstellar absorption lines in a sample of 10 star-forming galaxies at z similar to 0.2. Selected on the basis of high equivalent width optical emission lines, the sample, dubbed "Green Peas," make some of the best analogs for young galaxies in an early universe. We detect Ly alpha emission in all ten galaxies, and 9/10 show double-peaked line profiles suggestive of low H (I) column density. We measure Ly alpha/H alpha flux ratios of 0.5-5.6, implying that 5%-60% of Lya photons escape the galaxies. These data confirm previous findings that low-ionization metal absorption (LIS) lines are weaker when Ly alpha escape fraction and equivalent width are higher. However, contrary to previously favored interpretations of this trend, increased Ly alpha output cannot be the result of a varying H (I) covering: the Lyman absorption lines (Ly beta and higher) show a covering fraction near unity for gas with N-H I greater than or similar to 10(16) cm(-2). Moreover, we detect no correlation between Ly alpha escape and the outflow velocity of the LIS lines, suggesting that kinematic effects do not explain the range of Ly alpha/H alpha flux ratios in these galaxies. In contrast, we detect a strong anticorrelation between the Ly alpha escape fraction and the velocity separation of the Ly alpha emission peaks, driven primarily by the velocity of the blue peak. As this velocity separation is sensitive to H (I) column density, we conclude that Ly alpha escape in these Green Peas is likely regulated by the H (I) column density rather than outflow velocity or H (I) covering fraction.
C1 [Henry, Alaina] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Scarlata, Claudia] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Martin, Crystal L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Erb, Dawn] Univ Wisconsin, Dept Phys, Milwaukee, WI 53211 USA.
RP Henry, A (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
EM alaina.henry@nasa.gov
FU HST [GO 12928]; NSF [AST-1109288]; NSF CAREER grant [AST-1255591]
FX We acknowledge Marc Rafelski, Sanchayeeta Borthakur, Tucker Jones, Amber
Straughn, and Jonathan Gardner for helpful discussions. A.H. is
supported by HST GO 12928 and an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. C.L.M.
acknowledges partial support from NSF AST-1109288. D.K.E. acknowledges
support from NSF CAREER grant AST-1255591. 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. A.H.
and C.S. also acknowledge travel support and gracious hosting from the
Nordic Institute for Theoretical Physics during their program, Ly alpha
as an Astrophysical Tool.
NR 83
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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 AUG 10
PY 2015
VL 809
IS 1
AR 19
DI 10.1088/0004-637X/809/1/19
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500019
ER
PT J
AU Janches, D
Close, S
Hormaechea, JL
Swarnalingam, N
Murphy, A
O'Connor, D
Vandepeer, B
Fuller, B
Fritts, DC
Brunini, C
AF Janches, D.
Close, S.
Hormaechea, J. L.
Swarnalingam, N.
Murphy, A.
O'Connor, D.
Vandepeer, B.
Fuller, B.
Fritts, D. C.
Brunini, C.
TI THE SOUTHERN ARGENTINA AGILE METEOR RADAR ORBITAL SYSTEM (SAAMER-OS): AN
INITIAL SPORADIC METEOROID ORBITAL SURVEY IN THE SOUTHERN SKY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE meteorites, meteors, meteoroids; techniques: radar astronomy; zodiacal
dust
ID HEAD ECHO OBSERVATIONS; RADIO METEORS; VELOCITY DISTRIBUTION;
STATISTICAL-MODEL; EARTHS ATMOSPHERE; VIDEO METEORS; GREENLAND ICE;
SMOKE FALLOUT; SOLAR-SYSTEM; COSMIC DUST
AB We present an initial survey in the southern sky of the sporadic meteoroid orbital environment obtained with the Southern Argentina Agile MEteor Radar (SAAMER) Orbital System (OS), in which over three-quarters of a million orbits of dust particles were determined from 2012 January through 2015 April. SAAMER-OS is located at the southernmost tip of Argentina and is currently the only operational radar with orbit determination capability providing continuous observations of the southern hemisphere. Distributions of the observed meteoroid speed, radiant, and heliocentric orbital parameters are presented, as well as those corrected by the observational biases associated with the SAAMER-OS operating parameters. The results are compared with those reported by three previous surveys performed with the Harvard Radio Meteor Project, the Advanced Meteor Orbit Radar, and the Canadian Meteor Orbit Radar, and they are in agreement with these previous studies. Weighted distributions for meteoroids above the thresholds for meteor trail electron line density, meteoroid mass, and meteoroid kinetic energy. are also considered. Finally, the minimum line density and kinetic energy weighting factors are found to be very suitable for meteroid applications. The outcomes of this work show that, given SAAMER's location, the system is ideal for providing crucial data to continuously study the South Toroidal and South Apex sporadic meteoroid apparent sources.
C1 [Janches, D.; Swarnalingam, N.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
[Close, S.] Stanford Univ, Dept Aeronaut & Astronaut, Space Environm & Satellite Syst Lab, Palo Alto, CA 94304 USA.
[Hormaechea, J. L.] Estn Astron Rio Grande, Rio Grande, Tierra Del Fueg, Argentina.
[Hormaechea, J. L.] Univ Nacl Tierra del Fuego, Tierra Del Fuego, Argentina.
[Swarnalingam, N.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Murphy, A.; O'Connor, D.; Vandepeer, B.; Fuller, B.] Genesis Software Pty Ltd, Adelaide, SA, Australia.
[Fritts, D. C.] GATS Inc, Boulder, CO USA.
[Brunini, C.] Univ Nacl La Plata, Dept Astron & Geofis, La Plata, Buenos Aires, Argentina.
RP Janches, D (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Mail Code 674, Greenbelt, MD 20771 USA.
EM diego.janches@nasa.gov; sigridc@stanford.edu; jlhormaechea@untdf.edu.ar;
nimalan.swarnalingam@nasa.gov; amurphy@gsoft.com.au;
doconnor@gsoft.com.au; bvandepe@gsoft.com.au; bfuller@gsoft.com.au;
dave@gats-inc.com; claudiobrunini@yahoo.com
RI Janches, Diego/D-4674-2012;
OI Janches, Diego/0000-0001-8615-5166; Hormaechea, Jose
Luis/0000-0003-4533-3282
FU NSF [AGS-0634650, AGS-0944104, AST-0908118]; NASA [12-PAST12-0007,
12-PATM12-0006]
FX The deployment of SAAMER and its remote receiving stations, as well as
the work presented in this paper, were supported by NSF awards
AGS-0634650, AGS-0944104, and AST-0908118. D.J.'s participation is
currently supported through NASA awards 12-PAST12-0007 and
12-PATM12-0006. The authors wish to give special thanks to the EARG
personnel for their invaluable assistance with the operation and
day-to-day oversight of SAAMER. Without their help, operating a system
on the other side of the planet would be impossible! The authors wish to
thank Prof. Peter Brown for invaluable guidance for the final SAAMER-OS
design and deployment. Finally, the authors wish to acknowledge S. Pifko
for his work in determining SAAMER-OS orbits. Unfortunately, following
editorial rules, we could not include him as an author because, despite
numerous efforts to communicate with him, he has stopped answering us
and did not confirm his approval to be included as an author.
NR 74
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U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2015
VL 809
IS 1
AR 36
DI 10.1088/0004-637X/809/1/36
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500036
ER
PT J
AU Kitiashvili, IN
Kosovichev, AG
Mansour, NN
Wray, AA
AF Kitiashvili, I. N.
Kosovichev, A. G.
Mansour, N. N.
Wray, A. A.
TI REALISTIC MODELING OF LOCAL DYNAMO PROCESSES ON THE SUN
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dynamo; magnetohydrodynamics (MHD); methods: numerical; Sun: magnetic
fields; Sun: photosphere; turbulence
ID MAGNETIC PRANDTL NUMBERS; SCALE TURBULENT DYNAMO; QUIET SOLAR
ATMOSPHERE; NUMERICAL SIMULATIONS; CONDUCTING FLUID; SURFACE DYNAMO;
VORTEX TUBES; FIELDS; INTERNETWORK; CONVECTION
AB Magnetic fields are usually observed in the quiet Sun as small-scale elements that cover the entire solar surface (the "salt-and-pepper" patterns in line-of-sight magnetograms). By using 3D radiative MHD numerical simulations, we find that these fields result from a local dynamo action in the top layers of the convection zone, where extremely weak "seed" magnetic fields (e.g., from a 10-6 G) can locally grow above the mean equipartition field to a stronger than 2000 G field localized in magnetic structures. Our results reveal that the magnetic flux is predominantly generated in regions of small-scale helical downflows. We find that the local dynamo action takes place mostly in a shallow, about 500 km deep, subsurface layer, from which the generated field is transported into the deeper layers by convective downdrafts. We demonstrate that the observed dominance of vertical magnetic fields at the photosphere and horizontal fields above the photosphere can be explained by small-scale magnetic loops produced by the dynamo. Such small-scale loops play an important role in the structure and dynamics of the solar atmosphere and their detection in observations is critical for understanding the local dynamo action on the Sun.
C1 [Kitiashvili, I. N.; Mansour, N. N.; Wray, A. A.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Kosovichev, A. G.] New Jersey Inst Technol, Newark, NJ 07102 USA.
RP Kitiashvili, IN (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
EM irina.n.kitiashvili@nasa.gov
OI Kitiashvili, Irina/0000-0003-4144-2270
FU NASA [NNX10AC55G, NNH11ZDA001N-LWSCSW]; Oak Ridge Associated
Universities
FX The simulation results were obtained on NASA's Pleiades supercomputer at
NASA Ames Research Center. This work was partially supported by NASA
grants NNX10AC55G and NNH11ZDA001N-LWSCSW, and Oak Ridge Associated
Universities.
NR 81
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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 AUG 10
PY 2015
VL 809
IS 1
AR 84
DI 10.1088/0004-637X/809/1/84
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500084
ER
PT J
AU Machacek, JR
Mahapatra, DP
Schultz, DR
Ralchenko, Y
Moradmand, A
El Ghazaly, MOA
Chutjian, A
AF Machacek, J. R.
Mahapatra, D. P.
Schultz, D. R.
Ralchenko, Yu.
Moradmand, A.
El Ghazaly, M. O. A.
Chutjian, A.
TI SOLAR-WIND ION-DRIVEN X-RAY EMISSION FROM COMETARY AND PLANETARY
ATMOSPHERES: MEASUREMENTS AND THEORETICAL PREDICTIONS OF CHARGE-EXCHANGE
CROSS-SECTIONS AND EMISSION SPECTRA FOR O6+ + H2O, CO, CO2, CH4, N-2,
NO, N2O, AND Ar
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atomic processes; comets: general; molecular processes; solar wind
ID ATOMIC-HYDROGEN; IONIZATION; IMPACT; DISCOVERY
AB Relevant to modeling and understanding X-ray emission from cometary and planetary atmospheres, total cross-sections for 1.17 and 2.33 keV/u O6+ colliding with H2O, CO, CO2, CH4, N-2, NO, N2O, and Ar have been measured for the processes of single, double, and triple charge exchanges. Using these measurements as benchmarks, synthetic emission spectra spanning the X-ray, UV, and visible range have been calculated based on theoretical treatment of the transfer of between one and six electrons from the target neutrals to the projectile ion, followed by radiative and non-radiative decay of the highly excited states produced in these collisions. The results help add to the base of knowledge required to simulate ion-neutral processes in astrophysical environments; refine the present understanding of these fundamental atomic processes; and guide future observations, laboratory measurements, and theoretical predictions.
C1 [Machacek, J. R.] Australian Natl Univ, Res Sch Phys & Engn, Atom & Mol Phys Lab, Canberra, ACT 2601, Australia.
[Mahapatra, D. P.] Utkal Univ, Dept Phys, Bhubaneswar 751004, Orissa, India.
[Schultz, D. R.] Univ N Texas, Dept Phys, Denton, TX 76203 USA.
[Ralchenko, Yu.] NIST, Atom Spect Grp, Gaithersburg, MD 20899 USA.
[Moradmand, A.; El Ghazaly, M. O. A.; Chutjian, A.] CALTECH, Jet Prop Lab, Astrophys & Space Sci Sect, Pasadena, CA 91109 USA.
RP Machacek, JR (reprint author), Australian Natl Univ, Res Sch Phys & Engn, Atom & Mol Phys Lab, Canberra, ACT 2601, Australia.
RI Ralchenko, Yuri/E-9297-2016; Machacek, Joshua/A-5316-2011
OI Ralchenko, Yuri/0000-0003-0083-9554;
FU National Aeronautics and Space Administration
FX We thank Prof. R. Mawhorter for a helpful discussion on SW abundances.
The experimental research was carried out at JPL/Caltech under contract
with the National Aeronautics and Space Administration.
NR 38
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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 AUG 10
PY 2015
VL 809
IS 1
AR 75
DI 10.1088/0004-637X/809/1/75
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500075
ER
PT J
AU Valencic, LA
Smith, RK
AF Valencic, Lynne A.
Smith, Randall K.
TI INTERSTELLAR DUST PROPERTIES FROM A SURVEY OF X-RAY HALOS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; X-rays: ISM
ID COLOR-MAGNITUDE DIAGRAMS; GLOBULAR-CLUSTER SYSTEM; PULSAR 4U 1538-52;
SOURCE CYGNUS X-2; OPTICAL COUNTERPART; NEUTRON-STAR; CENTAURUS X-3;
BLACK-HOLE; METAL-RICH; GRS 1915+105
AB Interstellar dust grains produce X-ray halos around bright sources due to small-angle X-ray scattering. Numerous studies have examined these halos, but no systematic study has yet tested the available halo data against the large number of well-defined dust models in circulation. We have therefore obtained the largest sample to date of X-ray dust halos from XMM-Newton and Chandra, and fitted them with 14 commonly used dust grain models, including comparisons with the optical extinction, A(V), where available in the literature. Our main conclusions are summarized as follows. (1) Comparing A(V) with N-H values measured via X-ray spectral fits, we find a ratio of A(V)/N-H (10(21) cm(-2)) = 0.48 +/- 0.06, in agreement with previous work. (2) Out of 35 halos, 27 could be fit by one or more grain models, with the most successful models having maximum grain radius a(max) < 0.4 mu m and fewer large grains than the less successful models. This suggests that the diffuse ISM does not contain a signicant presence of grains with a(max) > 0.5 mu m. (3) Most halos were best fit assuming a single dust cloud dominated the scattering, rather than smoothly distributed dust along the sightline. (4) Eight sources could not be fit with the models considered here, most of which were along distant (d > 5 kpc) sight lines through the Galactic thin disk. (5) Some sight lines had halos with observed X-ray scattering optical depth tau(sca)/AV that were signicantly different than expected. This may result from an inhomogeneous dust distribution across the halo extraction area.
C1 [Valencic, Lynne A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Valencic, Lynne A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Smith, Randall K.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Valencic, LA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM lynne.a.valencic@nasa.gov
FU NASA [NNX10AE04G, NNX10AD10G]; Chandra grant [GO7-8142B]
FX The authors thank the anonymous referee for many insightful comments
that significantly improved this work. They also gratefully acknowledge
helpful discussions with Eli Dwek and Fred Seward. Financial support for
this work was made possible by NASA Grants NNX10AE04G and NNX10AD10G and
Chandra grant GO7-8142B.
NR 146
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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 AUG 10
PY 2015
VL 809
IS 1
AR 66
DI 10.1088/0004-637X/809/1/66
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500066
ER
PT J
AU Welsh, WF
Orosz, JA
Short, DR
Cochran, WD
Endl, M
Brugamyer, E
Haghighipour, N
Buchhave, LA
Doyle, LR
Fabrycky, DC
Hinse, TC
Kane, SR
Kostov, V
Mazeh, T
Mills, SM
Muller, TWA
Quarles, B
Quinn, SN
Ragozzine, D
Shporer, A
Steffen, JH
Tal-Or, L
Torres, G
Windmiller, G
Borucki, WJ
AF Welsh, William F.
Orosz, Jerome A.
Short, Donald R.
Cochran, William D.
Endl, Michael
Brugamyer, Erik
Haghighipour, Nader
Buchhave, Lars A.
Doyle, Laurance R.
Fabrycky, Daniel C.
Hinse, Tobias Cornelius
Kane, Stephen R.
Kostov, Veselin
Mazeh, Tsevi
Mills, Sean M.
Mueller, Tobias W. A.
Quarles, Billy
Quinn, Samuel N.
Ragozzine, Darin
Shporer, Avi
Steffen, Jason H.
Tal-Or, Lev
Torres, Guillermo
Windmiller, Gur
Borucki, William J.
TI KEPLER 453 b-THE 10th KEPLER TRANSITING CIRCUMBINARY PLANET
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; binaries: eclipsing; planets and satellites: detection;
planets and satellites: dynamical evolution and stability; stars:
individual (KIC 9632895, Kepler-453)
ID MAIN-SEQUENCE STARS; CLOSE BINARY-SYSTEMS; LOW-MASS; LIGHT CURVES;
HIERARCHICAL TRIPLE; ECLIPSING BINARIES; ROTATION PERIODS; STELLAR
ROTATION; TIDAL EVOLUTION; HABITABLE ZONES
AB We present the discovery of Kepler-453 b, a 6.2 R-circle plus planet in a low-eccentricity, 240.5 day orbit about an eclipsing binary. The binary itself consists of a 0.94 and 0.195 M-circle dot pair of stars with an orbital period of 27.32 days. The plane of the planet's orbit is rapidly precessing, and its inclination only becomes sufficiently aligned with the primary star in the latter portion of the Kepler data. Thus three transits are present in the second half of the light curve, but none of the three conjunctions that occurred during the first half of the light curve produced observable transits. The precession period is similar to 103 years, and during that cycle, transits are visible only similar to 8.9% of the time. This has the important implication that for every system like Kepler-453 that we detect, there are similar to 11.5 circumbinary systems that exist but are not currently exhibiting transits. The planet's mass is too small to noticeably perturb the binary, and consequently its mass is not measurable with these data; however, our photodynamical model places a 1 sigma upper limit of 16 M-circle plus. With a period 8.8 times that of the binary, the planet is well outside the dynamical instability zone. It does, however, lie within the habitable zone of the binary, making it the third of 10 Kepler circumbinary planets to do so.
C1 [Welsh, William F.; Orosz, Jerome A.; Short, Donald R.; Windmiller, Gur] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Cochran, William D.; Endl, Michael; Brugamyer, Erik] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
[Buchhave, Lars A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Doyle, Laurance R.] SETI Inst, Mountain View, CA 94043 USA.
[Doyle, Laurance R.] Principia Coll, IMoP, Elsah, IL 62028 USA.
[Fabrycky, Daniel C.; Mills, Sean M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Hinse, Tobias Cornelius] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Hinse, Tobias Cornelius] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Kane, Stephen R.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA.
[Kostov, Veselin] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Mazeh, Tsevi; Tal-Or, Lev] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Mueller, Tobias W. A.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Quarles, Billy; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
[Ragozzine, Darin] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Steffen, Jason H.] Northwestern Univ, CIERA, Evanston, IL 60208 USA.
[Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Orosz, JA (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA.
EM wwelsh@mail.sdsu.edu; jorosz@mail.sdsu.edu
OI Buchhave, Lars A./0000-0003-1605-5666
FU Institute for Astronomy; NASA Astrobiology Institute at the University
of Hawaii-Manoa; National Science Foundation [AST-1109928]; NASA's
Kepler Participating Scientist Program [NNX12AD23G]; Origins of Solar
Systems Program [NNX13AI76G]; Korea Research Council for Fundamental
Science and Technology (KRCF) through the Young Research Scientist
Fellowship Program; KASI (Korea Astronomy and Space Science Institute)
[2013-9-400-0/2014-1-400-06]; Northern Ireland Department of Culture,
Arts and Leisure (DCAL); NASA ADAP grant [NNX13AF20G]; NASA Origins
grant [NNX12AQ62G]; Astrobiology Institute under Institute for
Astronomy, University of Hawaii [NNA09DA77]; HST grant
[HST-GO-12548.06-A]; NASA from the Space Telescope Science Institute
[HST-GO-12548.06-A]; NASA [NAS5-26555]; European Research Council under
the EU's Seventh Framework Programme (ERC Grant) [291352]; NASA
Postdoctoral Program; NSF grant [AST-1007992]; NASA, Science Mission
Directorate
FX We thank the ApJ Editors for their patience and the anonymous referee
for suggestions that helped improve this paper. We thank Amy McQuillan
of Tel Aviv University for assistance with the measurement of the ACF,
and Justice Bruursema for assisting with the WIYN observations. W.F.W.
thanks the Institute for Astronomy and the NASA Astrobiology Institute
at the University of Hawaii-Manoa for their support and kind hospitality
during his sabbatical visit when part of this project was carried out.
W.F.W. and J.A.O. gratefully acknowledge support from the National
Science Foundation via grant AST-1109928, and from NASA's Kepler
Participating Scientist Program (NNX12AD23G) and Origins of Solar
Systems Program (NNX13AI76G). T.C.H. gratefully acknowledges financial
support from the Korea Research Council for Fundamental Science and
Technology (KRCF) through the Young Research Scientist Fellowship
Program and financial support from KASI (Korea Astronomy and Space
Science Institute) grant number 2013-9-400-0/2014-1-400-06. Numerical
computations were partly carried out using the SFI/HEA Irish Centre for
High-End Computing (ICHEC) and the KMTNet computing cluster at the Korea
Astronomy and Space Science Institute. Astronomical research at the
Armagh Observatory is funded by the Northern Ireland Department of
Culture, Arts and Leisure (DCAL). N.H. acknowledges support from the
NASA ADAP grant NNX13AF20G, NASA Origins grant NNX12AQ62G, Astrobiology
Institute under Cooperative Agreement NNA09DA77 at the Institute for
Astronomy, University of Hawaii, and HST grant HST-GO-12548.06-A.
Support for program HST-GO-12548.06-A 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. T.M. gratefully acknowledges support of
from the European Research Council under the EU's Seventh Framework
Programme (ERC Grant Agreement No. 291352). B.Q. gratefully acknowledges
the support of the NASA Postdoctoral Program. J.H.S. acknowledges the
support from NASA's Kepler Participating Scientist Program (NNX12AD23G).
G.T. acknowledges partial support from NSF grant AST-1007992. The
authors acknowledge the outstanding work of David Ciardi
(NExScI/Caltech) in organizing and maintaining the Kepler Community
Follow-up Observing Program (CFOP) website.26 We also thank
Phil Lucas for organizing the UKIRT J-band observations of the Kepler
field available on the CFOP website. 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. Kepler was
competitively selected as the 10th mission of the Discovery Program.
Funding for this mission is provided by NASA, Science Mission
Directorate.
NR 79
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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 AUG 10
PY 2015
VL 809
IS 1
AR 26
DI 10.1088/0004-637X/809/1/26
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CR9DN
UT WOS:000361653500026
ER
EF