FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Durack, PJ
   Gleckler, PJ
   Landerer, FW
   Taylor, KE
AF Durack, Paul J.
   Gleckler, Peter J.
   Landerer, Felix W.
   Taylor, Karl E.
TI Quantifying underestimates of long-term upper-ocean warming
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID SEA-LEVEL RISE; BUDGET; TRENDS
AB The global ocean stores more than 90% of the heat associated with observed greenhouse-gas-attributed global warming(1-4). Using satellite altimetry observations and a large suite of climate models, we conclude that observed estimates of 0-700 dbar global ocean warming since 1970 are likely biased low. This underestimation is attributed to poor sampling of the Southern Hemisphere, and limitations of the analysis methods that conservatively estimate temperature changes in data-sparse regions(5-7). We find that the partitioning of northern and southern hemispheric simulated sea surface height changes are consistent with precise altimeter observations, whereas the hemispheric partitioning of simulated upper-ocean warming is inconsistent with observed in-situ-based ocean heat content estimates. Relying on the close correspondence between hemispheric-scale ocean heat content and steric changes, we adjust the poorly constrained Southern Hemisphere observed warming estimates so that hemispheric ratios are consistent with the broad range of modelled results. These adjustments yield large increases (2.2-7.1 x 10(22) J 35 yr(-1)) to current global upper-ocean heat content change estimates, and have important implications for sea level, the planetary energy budget and climate sensitivity assessments.
C1 [Durack, Paul J.; Gleckler, Peter J.; Taylor, Karl E.] Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA 94550 USA.
   [Landerer, Felix W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Durack, PJ (reprint author), Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA 94550 USA.
EM pauldurack@llnl.gov
RI Taylor, Karl/F-7290-2011; Durack, Paul/A-8758-2010; 
OI Taylor, Karl/0000-0002-6491-2135; Durack, Paul/0000-0003-2835-1438;
   Landerer, Felix/0000-0003-2678-095X
FU US Department of Energy, Office of Science, Climate and Environmental
   Sciences Division, Regional and Global Climate Modeling Program
   [DE-AC52-07NA27344]; NASA ROSES Physical Oceanography [NNN13D462T]; NASA
   Sea Level Change Team (NSLCT)
FX The work of P.J.D., P.J.G. and K.E.T. from Lawrence Livermore National
   Laboratory is a contribution to the US Department of Energy, Office of
   Science, Climate and Environmental Sciences Division, Regional and
   Global Climate Modeling Program under contract DE-AC52-07NA27344. The
   work of F.W.L. was performed at the Jet Propulsion Laboratory,
   California Institute of Technology and is supported by NASA ROSES
   Physical Oceanography grant NNN13D462T and the NASA Sea Level Change
   Team (NSLCT). We thank numerous colleagues from the Program for Climate
   Model Diagnosis and Intercomparison (PCMDI) for valuable feedback and
   input into this project. We also thank J. Durack of the University of
   California, San Francisco (USA), M. V. Durack of educAID (Australia), T.
   P. Boyer from the National Oceanographic Data Center, Silver Spring
   (USA), C. M. Domingues from the Antarctic Climate and Ecosystems CRC,
   Hobart (Australia) and J. A. Church from the Centre for Australian
   Weather and Climate Research, Hobart (Australia). We acknowledge the
   sources of observed data used in this study: D. Smith and J. Murphy
   (Smi07), C. M. Domingues (Dom08), M. Ishii and M. Kimoto (Ish09), S.
   Levitus and T. Boyer (Lev12) and the International Argo Program and the
   national programs that contribute to it. We acknowledge the World
   Climate Research Programmes Working Group on Coupled Modelling, which is
   responsible for CMIP, and we thank the climate modelling groups (listed
   in Supplementary Tables 1 and 2) for producing and making available
   their model output. For CMIP the US Department of Energys 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. The DW10
   data presented in this study can be downloaded from the CSIRO Ocean
   Change website at www.cmar.csiro.au/oceanchange. LLNL Release #:
   LLNL-JRNL-651841.
NR 30
TC 35
Z9 37
U1 3
U2 34
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
EI 1758-6798
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD NOV
PY 2014
VL 4
IS 11
BP 999
EP 1005
DI 10.1038/NCLIMATE2389
PG 7
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
   Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AT0AD
UT WOS:000344598400024
ER

PT J
AU Llovel, W
   Willis, JK
   Landerer, FW
   Fukumori, I
AF Llovel, W.
   Willis, J. K.
   Landerer, F. W.
   Fukumori, I.
TI Deep-ocean contribution to sea level and energy budget not detectable
   over the past decade
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID HEAT-CONTENT; RISE; ARGO
AB As the dominant reservoir of heat uptake in the climate system, the world's oceans provide a critical measure of global climate change. Here, we infer deep-ocean warming in the context of global sea-level rise and Earth's energy budget between January 2005 and December 2013. Direct measurements of ocean warming above 2,000 m depth explain about 32% of the observed annual rate of global mean sea-level rise. Over the entire water column, independent estimates of ocean warming yield a contribution of 0.77 +/- 0.28 mm yr(-1) in sea-level rise and agree with the upper-ocean estimate to within the estimated uncertainties. Accounting for additional possible systematic uncertainties, the deep ocean (below 2,000 m) contributes 0.13 +/- 0.72 mm yr(-1) to global sea-level rise and 0.08 +/- 0.43 Wm(2) to Earth's energy balance. The net warming of the ocean implies an energy imbalance for the Earth of 0.64 +/- 0.44 Wm(2) from 2005 to 2013.
C1 [Llovel, W.; Willis, J. K.; Landerer, F. W.; Fukumori, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Llovel, W.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn UCLA JIFRESS, Los Angeles, CA 90024 USA.
RP Llovel, W (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM william.llovel@jpl.nasa.gov
RI LLOVEL, William/G-6930-2016
FU Oak Ridge Associated Universities through the NASA Postdoctoral Program
   (NPP); UCLA-JIFRESSE
FX W.L. was supported by Oak Ridge Associated Universities through the NASA
   Postdoctoral Program (NPP) carried out by JPL, Caltech and is now
   supported by UCLA-JIFRESSE. The temperature and salinity data were
   collected and made freely available by the International Argo Program
   and the national programs that contribute to it. (www.argo.ucsd.edu,
   http://argo.jcommops.org). The Argo Program is part of the Global Ocean
   Observing System. The research of J.K.W., F.W.L. and I.F. was carried
   out at JPL, Caltech under a contract with the National Aeronautics and
   Space Administration.
NR 36
TC 37
Z9 39
U1 6
U2 47
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
EI 1758-6798
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD NOV
PY 2014
VL 4
IS 11
BP 1031
EP 1035
DI 10.1038/NCLIMATE2387
PG 5
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
   Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AT0AD
UT WOS:000344598400029
ER

PT J
AU Itoh, Y
   Oasa, Y
   Kudo, T
   Kusakabe, N
   Hashimoto, J
   Abe, L
   Brandner, W
   Brandt, TD
   Carson, JC
   Egner, S
   Feldt, M
   Grady, CA
   Guyon, O
   Hayano, Y
   Hayashi, M
   Hayashi, SS
   Henning, T
   Hodapp, KW
   Ishii, M
   Iye, M
   Janson, M
   Kandori, R
   Knapp, GR
   Kuzuhara, M
   Kwon, J
   Matsuo, T
   McElwain, MW
   Miyama, S
   Morino, JI
   Moro-Martin, A
   Nishimura, T
   Pyo, TS
   Serabyn, E
   Suenaga, T
   Suto, H
   Suzuki, R
   Takahashi, YH
   Takato, N
   Terada, H
   Thalmann, C
   Tomono, D
   Turner, EL
   Watanabe, M
   Wisniewski, J
   Yamada, T
   Mayama, S
   Currie, T
   Takami, H
   Usuda, T
   Tamura, M
AF Itoh, Yoichi
   Oasa, Yumiko
   Kudo, Tomoyuki
   Kusakabe, Nobuhiko
   Hashimoto, Jun
   Abe, Lyu
   Brandner, Wolfgang
   Brandt, Timothy D.
   Carson, Joseph C.
   Egner, Sebastian
   Feldt, Markus
   Grady, Carol A.
   Guyon, Olivier
   Hayano, Yutaka
   Hayashi, Masahiko
   Hayashi, Saeko S.
   Henning, Thomas
   Hodapp, Klaus W.
   Ishii, Miki
   Iye, Masanori
   Janson, Markus
   Kandori, Ryo
   Knapp, Gillian R.
   Kuzuhara, Masayuki
   Kwon, Jungmi
   Matsuo, Taro
   McElwain, Michael W.
   Miyama, Shoken
   Morino, Jun-Ichi
   Moro-Martin, Amaya
   Nishimura, Tetsuo
   Pyo, Tae-Soo
   Serabyn, Eugene
   Suenaga, Takuya
   Suto, Hiroshi
   Suzuki, Ryuji
   Takahashi, Yasuhiro H.
   Takato, Naruhisa
   Terada, Hiroshi
   Thalmann, Christian
   Tomono, Daigo
   Turner, Edwin L.
   Watanabe, Makoto
   Wisniewski, John
   Yamada, Toru
   Mayama, Satoshi
   Currie, Thayne
   Takami, Hideki
   Usuda, Tomonori
   Tamura, Motohide
TI Near-infrared polarimetry of the GG Tauri A binary system
SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS
LA English
DT Article
DE stars: individual (GG Tauri); stars: pre-main sequence; techniques: high
   angular resolution
ID CIRCUMBINARY DISK; CIRCUMSTELLAR DISK; RING; ACCRETION; DYNAMICS; IMAGES
AB A high angular resolution near-infrared image that shows the intensity of polarization for the GG Tau A binary system was obtained with the Subaru Telescope. The image shows a circumbinary disk scattering the light from the central binary. The azimuthal profile of the intensity of polarization for the circumbinary disk is roughly reproduced by a simple disk model with the Henyey-Greenstein phase function and the Rayleigh function, indicating there are small dust grains at the surface of the disk. Combined with a previous observation of the circumbinary disk, our image indicates that the gap structure in the circumbinary disk orbits counterclockwise, but material in the disk orbits clockwise. We propose that there is a shadow caused by material located between the central binary and the circumbinary disk. The separations and position angles of the stellar components of the binary in the past 20 yr are consistent with the binary orbit with a = 33.4 AU and e = 0.34.
C1 [Itoh, Yoichi] Univ Hyogo, Ctr Astron, Nishi Harima Astron Observ, Sayo, Hyogo 6795313, Japan.
   [Oasa, Yumiko] Saitama Univ, Fac Educ, Sakura, Saitama 3388570, Japan.
   [Kudo, Tomoyuki; Egner, Sebastian; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko S.; Ishii, Miki; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
   [Kusakabe, Nobuhiko; Hayashi, Masahiko; Iye, Masanori; Kandori, Ryo; Kwon, Jungmi; Morino, Jun-Ichi; Suto, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro H.; Takami, Hideki; Usuda, Tomonori; Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
   [Hashimoto, Jun; Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
   [Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange UMR 7293, F-06108 Nice 2, France.
   [Brandner, Wolfgang] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Brandt, Timothy D.; Janson, Markus; Knapp, Gillian R.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
   [Carson, Joseph C.; Feldt, Markus] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
   [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.
   [Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
   [Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
   [Miyama, Shoken] Hiroshima Univ, Higashihiroshima, Hiroshima 7398511, Japan.
   [Moro-Martin, Amaya] CAB CSIC INTA, Dept Astrophys, Madrid 28850, Spain.
   [Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Suenaga, Takuya] Grad Univ Adv Studies, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
   [Takahashi, Yasuhiro H.; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
   [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.
   [Mayama, Satoshi] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan.
   [Currie, Thayne] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Itoh, Y (reprint author), Univ Hyogo, Ctr Astron, Nishi Harima Astron Observ, 407-2 Nishigaichi, Sayo, Hyogo 6795313, Japan.
EM yitoh@nhao.jp
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
FU U.S. National Science Foundation [1009203];  [24540231]
FX We thank Dr. Michihiro Takami for a useful discussion. Y. I. is
   supported by a Grant-in-Aid for Scientific Research (No. 24540231). J.
   C. is supported by the U.S. National Science Foundation under Award (No.
   1009203).
NR 26
TC 4
Z9 4
U1 1
U2 3
PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES
PI BEIJING
PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA
SN 1674-4527
J9 RES ASTRON ASTROPHYS
JI Res. Astron. Astrophys.
PD NOV
PY 2014
VL 14
IS 11
BP 1438
EP 1446
DI 10.1088/1674-4527/14/11/007
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT0BG
UT WOS:000344601200007
ER

PT J
AU Yashiro, S
   Gopalswamy, N
   Makela, P
   Akiyama, S
   Uddin, W
   Srivastava, AK
   Joshi, NC
   Chandra, R
   Manoharan, PK
   Mahalakshmi, K
   Dwivedi, VC
   Jain, R
   Awasthi, AK
   Nitta, NV
   Aschwanden, MJ
   Choudhary, DP
AF Yashiro, S.
   Gopalswamy, N.
   Maekelae, P.
   Akiyama, S.
   Uddin, W.
   Srivastava, A. K.
   Joshi, N. C.
   Chandra, R.
   Manoharan, P. K.
   Mahalakshmi, K.
   Dwivedi, V. C.
   Jain, R.
   Awasthi, A. K.
   Nitta, N. V.
   Aschwanden, M. J.
   Choudhary, D. P.
TI Homologous flare-CME events and their metric type II radio burst
   association
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Flares; CMEs; Shocks; Radio emission
ID CORONAL MASS EJECTIONS; DYNAMICS-OBSERVATORY SDO; SHOCK; EMISSION;
   BUILDUP; SUN
AB Active region NOAA 11158 produced many flares during its disk passage. At least two of these flares can be considered as homologous: the C6.6 flare at 06:51 UT and C9.4 flare at 12:41 UT on February 14, 2011. Both flares occurred at the same location (eastern edge of the active region) and have a similar decay of the GOES soft X-ray light curve. The associated coronal mass ejections (CMEs) were slow (334 and 337 km/s) and of similar apparent widths (43 degrees and 44 degrees), but they had different radio signatures. The second event was associated with a metric type II burst while the first one was not. The COR1 coronagraphs on board the STEREO spacecraft clearly show that the second CME propagated into the preceding CME that occurred 50 min before. These observations suggest that CME CME interaction might be a key process in exciting the type II radio emission by slow CMEs. (C)2014 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Yashiro, S.; Maekelae, P.; Akiyama, S.] Catholic Univ Amer, Washington, DC 20064 USA.
   [Yashiro, S.; Gopalswamy, N.; Maekelae, P.; Akiyama, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Uddin, W.; Awasthi, A. K.] ARIES Nainital, Naini Tal 263129, India.
   [Srivastava, A. K.] Indian Inst Technol BHU, Dept Phys, Varanasi 221005, Uttar Pradesh, India.
   [Chandra, R.] Kumaun Univ, Dept Phys, Naini Tal 263002, India.
   [Manoharan, P. K.; Mahalakshmi, K.; Dwivedi, V. C.] TIFR NCRA Radio Astron Ctr, Ootacamund 643001, India.
   [Awasthi, A. K.] Phys Res Lab, Ahmadabad 380009, Gujarat, India.
   [Nitta, N. V.; Aschwanden, M. J.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
   [Choudhary, D. P.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA.
   [Joshi, N. C.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea.
   [Jain, R.] Kadi Sarva Vishwavidyalaya, Gandhinagar 382015, Gujarat, India.
RP Yashiro, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM seiji.yashiro@nasa.gov
RI Awasthi, Arun/H-5596-2016
OI Awasthi, Arun/0000-0001-5313-1125
FU NASA LWS TRT program
FX This study was conducted as a part of the Indo-US Science and Technology
   Forum's Joint Center on Solar Eruptive Events. Part of the work is also
   supported by NASA LWS TR&T program.
NR 37
TC 4
Z9 4
U1 0
U2 3
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 NOV 1
PY 2014
VL 54
IS 9
BP 1941
EP 1948
DI 10.1016/j.asr.2014.07.002
PG 8
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
   Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA AS3UT
UT WOS:000344204200020
ER

PT J
AU Andreadis, KM
   Schumann, GJP
AF Andreadis, Konstantinos M.
   Schumann, Guy J-P.
TI Estimating the impact of satellite observations on the predictability of
   large-scale hydraulic models
SO ADVANCES IN WATER RESOURCES
LA English
DT Article
DE Hydraulic modeling; Forecasting; Data assimilation; Remote sensing;
   Floods; Large-scale
ID DATA-ASSIMILATION SYSTEM; ENSEMBLE KALMAN FILTER; OHIO RIVER-BASIN;
   SEQUENTIAL ASSIMILATION; FLOOD EXTENT; WATER LEVELS; ALTIMETRY; SCHEME
AB Large-scale hydraulic models are able to predict flood characteristics, and are being used in forecasting applications. In this work, the potential value of satellite observations to initialize hydraulic forecasts is explored, using the Ensemble Sensitivity method. The impact estimation is based on the Local Ensemble Transform Kalman Filter, allowing for the forecast error reductions to be computed without additional model runs. The experimental design consisted of two configurations of the LISFLOOD-FP model over the Ohio River basin: a baseline simulation represents a "best effort" model using observations for parameters and boundary conditions, whereas the second simulation consists of erroneous parameters and boundary conditions. Results showed that the forecast skill was improved for water heights up to lead times of 11 days (error reductions ranged from 0.2 to 0.6 m/km), while even partial observations of the river contained information for the entire river's water surface profile and allowed forecasting 5 to 7 days ahead. Moreover, water height observations had a negative impact on discharge forecasts for longer lead times although they did improve forecast skill for 1 and 3 days (up to 60 m(3)/s/km). Lastly, the inundated area forecast errors were reduced overall for all examined lead times. Albeit, when examining a specific flood event the limitations of predictability were revealed suggesting that model errors or inflows were more important than initial conditions. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Andreadis, Konstantinos M.; Schumann, Guy J-P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Andreadis, KM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kandread@jpl.nasa.gov
NR 53
TC 8
Z9 8
U1 2
U2 20
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 NOV
PY 2014
VL 73
BP 44
EP 54
DI 10.1016/j.advwatres.2014.06.006
PG 11
WC Water Resources
SC Water Resources
GA AS1US
UT WOS:000344068000004
ER

PT J
AU Rummel, JD
   Beaty, DW
   Jones, MA
   Bakermans, C
   Barlow, NG
   Boston, PJ
   Chevrier, VF
   Clark, BC
   de Vera, JPP
   Gough, RV
   Hallsworth, JE
   Head, JW
   Hipkin, VJ
   Kieft, TL
   McEwen, AS
   Mellon, MT
   Mikucki, JA
   Nicholson, WL
   Omelon, CR
   Peterson, R
   Roden, EE
   Sherwood Lollar, B
   Tanaka, KL
   Viola, D
   Wray, JJ
AF Rummel, John D.
   Beaty, David W.
   Jones, Melissa A.
   Bakermans, Corien
   Barlow, Nadine G.
   Boston, Penelope J.
   Chevrier, Vincent F.
   Clark, Benton C.
   de Vera, Jean-Pierre P.
   Gough, Raina V.
   Hallsworth, John E.
   Head, James W.
   Hipkin, Victoria J.
   Kieft, Thomas L.
   McEwen, Alfred S.
   Mellon, Michael T.
   Mikucki, Jill A.
   Nicholson, Wayne L.
   Omelon, Christopher R.
   Peterson, Ronald
   Roden, Eric E.
   Sherwood Lollar, Barbara
   Tanaka, Kenneth L.
   Viola, Donna
   Wray, James J.
TI A New Analysis of Mars "Special Regions": Findings of the Second MEPAG
   Special Regions Science Analysis Group (SR-SAG2)
SO ASTROBIOLOGY
LA English
DT News Item
ID ORBITER LASER ALTIMETER; RECURRING SLOPE LINEAE; CARBON-DIOXIDE
   EXCHANGE; MARTIAN IMPACT CRATERS; SEASONAL POLAR-CAP; WATER-VAPOR
   UPTAKE; VOSTOK ICE CORE; LITHOAUTOTROPHIC MICROBIAL ECOSYSTEMS;
   SPACECRAFT-ASSOCIATED MICROORGANISMS; SOIL HETEROTROPHIC RESPIRATION
AB A committee of the Mars Exploration Program Analysis Group (MEPAG) has reviewed and updated the description of Special Regions on Mars as places where terrestrial organisms might replicate (per the COSPAR Planetary Protection Policy). This review and update was conducted by an international team (SR-SAG2) drawn from both the biological science and Mars exploration communities, focused on understanding when and where Special Regions could occur. The study applied recently available data about martian environments and about terrestrial organisms, building on a previous analysis of Mars Special Regions (2006) undertaken by a similar team. Since then, a new body of highly relevant information has been generated from the Mars Reconnaissance Orbiter (launched in 2005) and Phoenix (2007) and data from Mars Express and the twin Mars Exploration Rovers (all 2003). Results have also been gleaned from the Mars Science Laboratory (launched in 2011). In addition to Mars data, there is a considerable body of new data regarding the known environmental limits to life on Earth-including the potential for terrestrial microbial life to survive and replicate under martian environmental conditions. The SR-SAG2 analysis has included an examination of new Mars models relevant to natural environmental variation in water activity and temperature; a review and reconsideration of the current parameters used to define Special Regions; and updated maps and descriptions of the martian environments recommended for treatment as "Uncertain" or "Special" as natural features or those potentially formed by the influence of future landed spacecraft. Significant changes in our knowledge of the capabilities of terrestrial organisms and the existence of possibly habitable martian environments have led to a new appreciation of where Mars Special Regions may be identified and protected. The SR-SAG also considered the impact of Special Regions on potential future human missions to Mars, both as locations of potential resources and as places that should not be inadvertently contaminated by human activity. Key Words: Martian environments-Mars astrobiology-Extreme environment microbiology-Planetary protection-Exploration resources. Astrobiology 14, 887-968.
C1 [Rummel, John D.] E Carolina Univ, Dept Biol, Greenville, NC 27858 USA.
   [Beaty, David W.; Jones, Melissa A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Bakermans, Corien] Penn State Univ, Altoona Coll, Altoona, PA USA.
   [Barlow, Nadine G.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA.
   [Boston, Penelope J.; Kieft, Thomas L.] New Mexico Inst Min & Technol, Socorro, NM USA.
   [Chevrier, Vincent F.] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA.
   [Clark, Benton C.] Space Sci Inst, Boulder, CO USA.
   [de Vera, Jean-Pierre P.] Inst Planetary Res, German Aerosp Ctr, Berlin, Germany.
   [Gough, Raina V.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
   [Hallsworth, John E.] Queens Univ Belfast, Sch Biol Sci, Inst Global Food Secur, Belfast, Antrim, North Ireland.
   [Head, James W.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
   [Hipkin, Victoria J.] Canadian Space Agcy, St Hubert, PQ, Canada.
   [McEwen, Alfred S.; Viola, Donna] Univ Arizona, Tucson, AZ USA.
   [Mellon, Michael T.] SW Res Inst, Boulder, CO USA.
   [Mikucki, Jill A.] Univ Tennessee, Dept Microbiol, Knoxville, TN 37996 USA.
   [Nicholson, Wayne L.] Univ Florida, Dept Microbiol & Cell Sci, Merritt Isl, FL USA.
   [Omelon, Christopher R.] Univ Texas Austin, Dept Geol Sci, Austin, TX USA.
   [Peterson, Ronald] Queens Univ, Kingston, ON, Canada.
   [Roden, Eric E.] Univ Wisconsin, Dept Geosci, Madison, WI USA.
   [Roden, Eric E.] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI USA.
   [Sherwood Lollar, Barbara] Univ Toronto, Toronto, ON, Canada.
   [Tanaka, Kenneth L.] US Geol Survey, Flagstaff, AZ 86001 USA.
   [Wray, James J.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
RP Rummel, JD (reprint author), E Carolina Univ, Dept Biol, ICSP, Flanagan 250, Greenville, NC 27858 USA.
EM rummelj@ecu.edu
RI Wray, James/B-8457-2008; Hallsworth, John/K-7876-2013; Mellon,
   Michael/C-3456-2016
OI Wray, James/0000-0001-5559-2179; 
NR 628
TC 51
Z9 51
U1 7
U2 73
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 NOV 1
PY 2014
VL 14
IS 11
BP 887
EP 968
DI 10.1089/ast.2014.1227
PG 82
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
   Geology
GA AT3XP
UT WOS:000344868500001
PM 25401393
ER

PT J
AU Jacobson, RA
AF Jacobson, R. A.
TI THE ORBITS OF THE URANIAN SATELLITES AND RINGS, THE GRAVITY FIELD OF THE
   URANIAN SYSTEM, AND THE ORIENTATION OF THE POLE OF URANUS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE planets and satellites: individual (Uranus); planets and satellites:
   rings
ID 1982 STELLAR OCCULTATION; ASTROMETRIC OBSERVATIONS; OUTER PLANETS;
   NATURAL SATELLITES; NUMERICAL-INTEGRATION; FASTT OBSERVATIONS; REFERENCE
   FRAME; POSITIONS; ECLIPSES; MOTION
AB French et al. determined the orbits of the Uranian rings, the orientation of the pole of Uranus, and the gravity harmonics of Uranus from Earth-based and Voyager ring occultations. Jacobson et al. determined the orbits of the Uranian satellites and the masses of Uranus and its satellites from Earth-based astrometry and observations acquired with the Voyager 2 spacecraft; they used the gravity harmonics and pole from French et al. Jacobson & Rush reconstructed the Voyager 2 trajectory and redetermined the Uranian system gravity parameters, satellite orbits, and ring orbits in a combined analysis of the data used previously augmented with additional Earth-based astrometry. Here we report on an extension of that work that incorporates additional astrometry and ring occultations together with improved data processing techniques.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jacobson, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM robert.jacobson@jpl.nasa.gov
NR 103
TC 4
Z9 4
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2014
VL 148
IS 5
AR 76
DI 10.1088/0004-6256/148/5/76
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS2YB
UT WOS:000344141200002
ER

PT J
AU Rebull, LM
   Cody, AM
   Covey, KR
   Gunther, HM
   Hillenbrand, LA
   Plavchan, P
   Poppenhaeger, K
   Stauffer, JR
   Wolk, SJ
   Gutermuth, R
   Morales-Calderon, M
   Song, I
   Barrado, D
   Bayo, A
   James, D
   Hora, JL
   Vrba, FJ
   de Oliveira, CA
   Bouvier, J
   Carey, SJ
   Carpenter, JM
   Favata, F
   Flaherty, K
   Forbrich, J
   Hernandez, J
   McCaughrean, MJ
   Megeath, ST
   Micela, G
   Smith, HA
   Terebey, S
   Turner, N
   Allen, L
   Ardila, D
   Bouy, H
   Guieu, S
AF Rebull, L. M.
   Cody, A. M.
   Covey, K. R.
   Guenther, H. M.
   Hillenbrand, L. A.
   Plavchan, P.
   Poppenhaeger, K.
   Stauffer, J. R.
   Wolk, S. J.
   Gutermuth, R.
   Morales-Calderon, M.
   Song, I.
   Barrado, D.
   Bayo, A.
   James, D.
   Hora, J. L.
   Vrba, F. J.
   de Oliveira, C. Alves
   Bouvier, J.
   Carey, S. J.
   Carpenter, J. M.
   Favata, F.
   Flaherty, K.
   Forbrich, J.
   Hernandez, J.
   McCaughrean, M. J.
   Megeath, S. T.
   Micela, G.
   Smith, H. A.
   Terebey, S.
   Turner, N.
   Allen, L.
   Ardila, D.
   Bouy, H.
   Guieu, S.
TI YOUNG STELLAR OBJECT VARIABILITY (YSOVAR): LONG TIMESCALE VARIATIONS IN
   THE MID-INFRARED
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE circumstellar matter; stars: pre-main sequence; stars: protostars;
   stars: variables: general
ID ORION-NEBULA-CLUSTER; T-TAURI STARS; MAIN-SEQUENCE STARS;
   SPITZER-SPACE-TELESCOPE; LOW-MASS STARS; ROTATION PERIOD DISTRIBUTION;
   NEAR-INFRARED VARIABILITY; OPHIUCHI MOLECULAR CLOUD; X-RAY OBSERVATIONS;
   NGC 2264
AB The YSOVAR (Young Stellar Object VARiability) Spitzer Space Telescope observing program obtained the first extensive mid-infrared (3.6 and 4.5 mu m) time series photometry of the Orion Nebula Cluster plus smaller footprints in 11 other star-forming cores (AFGL 490, NGC 1333, Mon R2, GGD 12-15, NGC 2264, L1688, Serpens Main, Serpens South, IRAS 20050+2720, IC 1396A, and Ceph C). There are similar to 29,000 unique objects with light curves in either or both IRAC channels in the YSOVAR data set. We present the data collection and reduction for the Spitzer and ancillary data, and define the "standard sample" on which we calculate statistics, consisting of fast cadence data, with epochs roughly twice per day for similar to 40 days. We also define a "standard sample of members" consisting of all the IR-selected members and X-ray-selected members. We characterize the standard sample in terms of other properties, such as spectral energy distribution shape. We use three mechanisms to identify variables in the fast cadence data-the Stetson index, a chi(2) fit to a flat light curve, and significant periodicity. We also identified variables on the longest timescales possible of six to seven years by comparing measurements taken early in the Spitzer mission with the mean from our YSOVAR campaign. The fraction of members in each cluster that are variable on these longest timescales is a function of the ratio of Class I/total members in each cluster, such that clusters with a higher fraction of Class I objects also have a higher fraction of long-term variables. For objects with a YSOVAR-determined period and a [3.6]-[8] color, we find that a star with a longer period is more likely than those with shorter periods to have an IR excess. We do not find any evidence for variability that causes [3.6]-[4.5] excesses to appear or vanish within our data set; out of members and field objects combined, at most 0.02% may have transient IR excesses.
C1 [Rebull, L. M.; Cody, A. M.; Stauffer, J. R.; Morales-Calderon, M.; Carey, S. J.] CALTECH, Spitzer Sci Ctr, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
   [Covey, K. R.] Lowell Observ, Flagstaff, AZ 86001 USA.
   [Guenther, H. M.; Poppenhaeger, K.; Wolk, S. J.; Hora, J. L.; Forbrich, J.; Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Hillenbrand, L. A.; Carpenter, J. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
   [Plavchan, P.] CALTECH, NASA Exoplanet Sci Inst NExScI, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
   [Plavchan, P.] Missouri State Univ, Springfield, MO 65897 USA.
   [Gutermuth, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
   [Morales-Calderon, M.; Barrado, D.; Bouy, H.] INTA CSIC, Ctr Astrobiol, Dept Astrofis, E-28691 Villanueva De La Canada, Spain.
   [Song, I.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
   [Bayo, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Bayo, A.] Univ Valparaiso, Fac Ciencias, Dept Fis & Astron, Valparaiso, Chile.
   [James, D.] Cerro Tololo InterAmer Observ, La Serena, Chile.
   [Vrba, F. J.] US Naval Observ, Flagstaff, AZ 86005 USA.
   [de Oliveira, C. Alves] European Space Agcy ESA ESAC, E-28691 Madrid, Spain.
   [Bouvier, J.; Guieu, S.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
   [Bouvier, J.] CNRS, IPAG, F-38000 Grenoble, France.
   [Favata, F.; McCaughrean, M. J.] European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands.
   [Flaherty, K.] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA.
   [Forbrich, J.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria.
   [Hernandez, J.] Ctr Invest Astron, Merida 5101A, Venezuela.
   [Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Ritter Astrophys Observ, Toledo, OH 43606 USA.
   [Micela, G.] INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy.
   [Terebey, S.] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90032 USA.
   [Turner, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Allen, L.] Natl Opt Astron Observ, Tucson, AZ USA.
   [Ardila, D.] CALTECH, NASA Herschel Sci Ctr NHSC, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
RP Rebull, LM (reprint author), CALTECH, Spitzer Sci Ctr, Infrared Proc & Anal Ctr, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
EM rebull@ipac.caltech.edu
RI Bouy, Herve/H-2913-2012; Barrado Navascues, David/C-1439-2017;
   Morales-Calderon, Maria/C-8384-2017; 
OI Covey, Kevin/0000-0001-6914-7797; Bouy, Herve/0000-0002-7084-487X;
   Barrado Navascues, David/0000-0002-5971-9242; Morales-Calderon,
   Maria/0000-0001-9526-9499; Micela, Giuseppina/0000-0002-9900-4751;
   Poppenhaeger, Katja/0000-0003-1231-2194; Gunther, Hans
   Moritz/0000-0003-4243-2840; Rebull, Luisa/0000-0001-6381-515X
NR 139
TC 33
Z9 33
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2014
VL 148
IS 5
AR 92
DI 10.1088/0004-6256/148/5/92
PG 46
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS2YB
UT WOS:000344141200018
ER

PT J
AU Wright, EL
   Mainzer, A
   Kirkpatrick, JD
   Masci, F
   Cushing, MC
   Bauer, J
   Fajardo-Acosta, S
   Gelino, CR
   Beichman, CA
   Skrutskie, MF
   Grav, T
   Eisenhardt, PRM
   Cutri, R
AF Wright, Edward L.
   Mainzer, Amy
   Kirkpatrick, J. Davy
   Masci, Frank
   Cushing, Michael C.
   Bauer, James
   Fajardo-Acosta, Sergio
   Gelino, Christopher R.
   Beichman, Charles A.
   Skrutskie, M. F.
   Grav, T.
   Eisenhardt, Peter R. M.
   Cutri, Roc
TI NEOWISE-R OBSERVATION OF THE COOLEST KNOWN BROWN DWARF
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE astrometry; brown dwarfs; infrared: stars; solar neighborhood; stars:
   individual (WISE J085510.83-071442.5); stars: low-mass
ID SPITZER-SPACE-TELESCOPE; ADAPTIVE OPTICS SYSTEM; PERFORMANCE; MISSION
AB The Wide-field Infrared Survey Explorer (WISE) spacecraft has been reactivated as NEOWISE-R to characterize and search for near-Earth objects. The brown dwarf WISE J085510.83-071442.5 has now been re-observed by NEOWISE-R, and we confirm the results of Luhman, who found a very low effective temperature (approximate to 250 K), a very high proper motion (8 ''.1 +/- 0 ''.1 yr(-1)), and a large parallax (454 +/- 45 mas). The large proper motion has separated the brown dwarf from the background sources that influenced the 2010 WISE data, allowing a measurement of a very red WISE color of W1 - W2 > 3.9 mag. A re-analysis of the 2010 WISE astrometry using only the W2 band, combined with the new NEOWISE-R 2014 position, gives an improved parallax of 448 +/- 33 mas and a proper motion of 8 ''.08 +/- 0 ''.05 yr(-1). These are all consistent with values from Luhman.
C1 [Wright, Edward L.] UCLA Astron, Los Angeles, CA 90095 USA.
   [Mainzer, Amy; Bauer, James; Eisenhardt, Peter R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Kirkpatrick, J. Davy; Masci, Frank; Fajardo-Acosta, Sergio; Gelino, Christopher R.; Beichman, Charles A.; Cutri, Roc] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
   [Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
   [Beichman, Charles A.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
   [Skrutskie, M. F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
   [Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
RP Wright, EL (reprint author), UCLA Astron, POB 951547, Los Angeles, CA 90095 USA.
EM wright@astro.ucla.edu
FU 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 makes use of data products from
   NEOWISE, which is a project of the Jet Propulsion Laboratory/California
   Institute of Technology, funded by the National Aeronautics and Space
   Administration.
NR 17
TC 11
Z9 11
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2014
VL 148
IS 5
AR 82
DI 10.1088/0004-6256/148/5/82
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS2YB
UT WOS:000344141200008
ER

PT J
AU Sana, H
   Le Bouquin, JB
   Lacour, S
   Berger, JP
   Duvert, G
   Gauchet, L
   Norris, B
   Olofsson, J
   Pickel, D
   Zins, G
   Absil, O
   de Koter, A
   Kratter, K
   Schnurr, O
   Zinnecker, H
AF Sana, H.
   Le Bouquin, J. -B.
   Lacour, S.
   Berger, J. -P.
   Duvert, G.
   Gauchet, L.
   Norris, B.
   Olofsson, J.
   Pickel, D.
   Zins, G.
   Absil, O.
   de Koter, A.
   Kratter, K.
   Schnurr, O.
   Zinnecker, H.
TI SOUTHERN MASSIVE STARS AT HIGH ANGULAR RESOLUTION: OBSERVATIONAL
   CAMPAIGN AND COMPANION DETECTION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: visual; stars: early-type; stars: imaging; surveys;
   techniques: high angular resolution; techniques: interferometric
ID BASE-LINE INTERFEROMETRY; ULTRAVIOLET RADIAL-VELOCITIES; SPECTROSCOPIC
   BINARY ORBITS; YOUNG OPEN CLUSTERS; O-TYPE STARS; SPARSE APERTURE
   MASKING; ORION NEBULA CLUSTER; X-MEGA TARGETS; GALACTIC-O; OPTICAL
   SPECTROSCOPY
AB Multiplicity is one of the most fundamental observable properties of massive O-type stars and offers a promising way to discriminate between massive star formation theories. Nevertheless, companions at separations between 1 and 100 milliarcsec (mas) remain mostly unknown due to intrinsic observational limitations. At a typical distance of 2 kpc, this corresponds to projected physical separations of 2-200 AU. The Southern MAssive Stars at High angular resolution survey (smash+) was designed to fill this gap by providing the first systematic interferometric survey of Galactic massive stars. We observed 117 O-type stars with VLTI/PIONIER and 162 O-type stars with NACO/Sparse Aperture Masking (SAM), probing the separation ranges 1-45 and 30-250 mas and brightness contrasts of Delta H < 4 and Delta H < 5, respectively. Taking advantage of NACO's field of view, we further uniformly searched for visual companions in an 8 '' radius down to Delta H = 8. This paper describes observations and data analysis, reports the discovery of almost 200 new companions in the separation range from 1 mas to 8 '' and presents a catalog of detections, including the first resolved measurements of over a dozen known long-period spectroscopic binaries. Excluding known runaway stars for which no companions are detected, 96 objects in our main sample (delta < 0 degrees; H < 7.5) were observed both with PIONIER and NACO/SAM. The fraction of these stars with at least one resolved companion within 200 mas is 0.53. Accounting for known but unresolved spectroscopic or eclipsing companions, the multiplicity fraction at separation rho < 8 '' increases to f(m) = 0.91 +/- 0.03. The fraction of luminosity class V stars that have a bound companion reaches 100% at 30 mas while their average number of physically connected companions within 8 '' is f(c) = 2.2 +/- 0.3. This demonstrates that massive stars form nearly exclusively in multiple systems. The nine non-thermal radio emitters observed by smash+ are all resolved, including the newly discovered pairs HD 168112 and CPD-47 degrees 2963. This lends strong support to the universality of the wind-wind collision scenario to explain the non-thermal emission from O-type stars.
C1 [Sana, H.] European Space Agcy, Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Le Bouquin, J. -B.; Duvert, G.; Zins, G.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
   [Le Bouquin, J. -B.; Duvert, G.; Zins, G.] CNRS, IPAG, F-38000 Grenoble, France.
   [Lacour, S.; Gauchet, L.; Pickel, D.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, F-92195 Meudon, France.
   [Berger, J. -P.] European So Observ, D-85748 Garching, Germany.
   [Norris, B.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
   [Olofsson, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Absil, O.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege, Belgium.
   [de Koter, A.] Univ Amsterdam, Astrophys Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
   [de Koter, A.] Univ Louvain, Inst Sterrenkunde, B-3001 Louvain, Belgium.
   [Kratter, K.] Univ Colorado, JILA, Boulder, CO 80309 USA.
   [Kratter, K.] Univ Arizona, Steward Observ, Dept Astron, Tucson, AZ 85721 USA.
   [Schnurr, O.] Leibniz Inst Astrophys Potsdam, D-14482 Potsdam, Germany.
   [Zinnecker, H.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Deutsch SOFIA Inst, Moffett Field, CA 94035 USA.
RP Sana, H (reprint author), European Space Agcy, Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM hsana@stsci.edu
RI Sana, Hugues/B-2664-2013; 
OI Sana, Hugues/0000-0001-6656-4130; Absil, Olivier/0000-0002-4006-6237
FU Universite Joseph Fourier (UJF); Institut de Planetologie et
   d'Astrophysique de Grenoble (IPAG); Agence Nationale pour la Recherche
   [ANR-06-BLAN-0421, ANR-10-BLAN-0505]; Institut National des Science de
   l'Univers (INSU PNPand PNPS); CNRS RT funding; NASA [HF-51306.01]; Space
   Telescope Science Institute
FX This work is based on observations collected at the European Southern
   Observatory under programs IDs 086.D-0641, 088.D-0579, 189.C-0644, and
   090.C-0672. PIONIER is funded by the Universite Joseph Fourier (UJF),
   the Institut de Planetologie et d'Astrophysique de Grenoble (IPAG), the
   Agence Nationale pour la Recherche (ANR-06-BLAN-0421 and
   ANR-10-BLAN-0505), and the Institut National des Science de l'Univers
   (INSU PNPand PNPS). The integrated optics beam combiner results from a
   collaboration between IPAG and CEA/LETI based on CNRS R&T funding.
   Support for K.M.K. was provided by NASA through Hubble Fellowship grant
   No. HF-51306.01 awarded by the Space Telescope Science Institute, which
   is operated by the Association of Universities for Research in
   Astronomy, Inc., for NASA, under contract NAS 5-26555. The authors
   warmly thank the people involved in the VLTI project as well a J. Maiz
   Apellaniz and B. Mason for constructive discussions and suggestions. We
   are also grateful to the referee for comments that improved the quality
   of the paper. We made use of the Smithsonian/NASA Astrophysics Data
   System (ADS), of the Centre de Donnees astronomiques de Strasbourg
   (CDS), and of the Washington Double Star Catalog (WDS), which is
   maintained at the U.S. Naval Observatory. Part of the calculations and
   graphics were performed with the freeware Yorick.
NR 113
TC 46
Z9 46
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2014
VL 215
IS 1
AR 15
DI 10.1088/0067-0049/215/1/15
PG 35
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS2YH
UT WOS:000344141800015
ER

PT J
AU Schwadron, NA
   Moebius, E
   Fuselier, SA
   McComas, DJ
   Funsten, HO
   Janzen, P
   Reisenfeld, D
   Kucharek, H
   Lee, MA
   Fairchild, K
   Allegrini, F
   Dayeh, M
   Livadiotis, G
   Reno, M
   Bzowski, M
   Sokol, JM
   Kubiak, MA
   Christian, ER
   DeMajistre, R
   Frisch, P
   Galli, A
   Wurz, P
   Gruntman, M
AF Schwadron, N. A.
   Moebius, E.
   Fuselier, S. A.
   McComas, D. J.
   Funsten, H. O.
   Janzen, P.
   Reisenfeld, D.
   Kucharek, H.
   Lee, M. A.
   Fairchild, K.
   Allegrini, F.
   Dayeh, M.
   Livadiotis, G.
   Reno, M.
   Bzowski, M.
   Sokol, J. M.
   Kubiak, M. A.
   Christian, E. R.
   DeMajistre, R.
   Frisch, P.
   Galli, A.
   Wurz, P.
   Gruntman, M.
TI SEPARATION OF THE RIBBON FROM GLOBALLY DISTRIBUTED ENERGETIC NEUTRAL
   ATOM FLUX USING THE FIRST FIVE YEARS OF IBEX OBSERVATIONS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE Sun: heliosphere; ISM: magnetic fields
ID INTERSTELLAR-BOUNDARY-EXPLORER; PICK-UP IONS; MAGNETIC-FIELD;
   SOLAR-WIND; OUTER HELIOSHEATH; VOYAGER 1; ENA FLUX; HELIOPAUSE;
   HELIOSPHERE; PLASMA
AB The Interstellar Boundary Explorer (IBEX) observes the IBEX ribbon, which stretches across much of the sky observed in energetic neutral atoms (ENAs). The ribbon covers a narrow (similar to 20 degrees-50 degrees) region that is believed to be roughly perpendicular to the interstellar magnetic field. Superimposed on the IBEX ribbon is the globally distributed flux that is controlled by the processes and properties of the heliosheath. This is a second study that utilizes a previously developed technique to separate ENA emissions in the ribbon from the globally distributed flux. A transparency mask is applied over the ribbon and regions of high emissions. We then solve for the globally distributed flux using an interpolation scheme. Previously, ribbon separation techniques were applied to the first year of IBEX-Hi data at and above 0.71 keV. Here we extend the separation analysis down to 0.2 keV and to five years of IBEX data enabling first maps of the ribbon and the globally distributed flux across the full sky of ENA emissions. Our analysis shows the broadening of the ribbon peak at energies below 0.71 keV and demonstrates the apparent deformation of the ribbon in the nose and heliotail. We show global asymmetries of the heliosheath, including both deflection of the heliotail and differing widths of the lobes, in context of the direction, draping, and compression of the heliospheric magnetic field. We discuss implications of the ribbon maps for the wide array of concepts that attempt to explain the ribbon's origin. Thus, we present the five-year separation of the IBEX ribbon from the globally distributed flux in preparation for a formal IBEX data release of ribbon and globally distributed flux maps to the heliophysics community.
C1 [Schwadron, N. A.; Moebius, E.; Kucharek, H.; Lee, M. A.; Fairchild, K.] Univ New Hampshire, Durham, NH 03824 USA.
   [Schwadron, N. A.; Fuselier, S. A.; Allegrini, F.; Dayeh, M.; Livadiotis, G.; Reno, M.] SW Res Inst, San Antonio, TX 78228 USA.
   [McComas, D. J.; Funsten, H. O.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
   [Janzen, P.; Reisenfeld, D.] Univ Montana, Missoula, MT 59812 USA.
   [Bzowski, M.; Sokol, J. M.; Kubiak, M. A.] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland.
   [Christian, E. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [DeMajistre, R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
   [Frisch, P.] Univ Chicago, Chicago, IL 60637 USA.
   [Galli, A.; Wurz, P.] Univ Bern, Bern, Switzerland.
   [Gruntman, M.] Univ So Calif, Los Angeles, CA 90089 USA.
   [Schwadron, N. A.] Univ Texas San Antonio, San Antonio, TX 78228 USA.
RP Schwadron, NA (reprint author), Univ New Hampshire, Durham, NH 03824 USA.
RI Funsten, Herbert/A-5702-2015; Reisenfeld, Daniel/F-7614-2015; Gruntman,
   Mike/A-5426-2008; Sokol, Justyna/K-2892-2015; 
OI Funsten, Herbert/0000-0002-6817-1039; Gruntman,
   Mike/0000-0002-0830-010X; Moebius, Eberhard/0000-0002-2745-6978
FU NASA's Explorer Program; Polish National Science Centre
   [2012-06-M-ST9-00455]
FX We are deeply indebted to all of the outstanding people who have made
   the IBEX mission possible. This work was carried out as a part of the
   IBEX project, with support from NASA's Explorer Program. J.S., M.B., and
   M.A.K. were supported by the Polish National Science Centre (grant
   2012-06-M-ST9-00455).
NR 52
TC 22
Z9 22
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2014
VL 215
IS 1
AR 13
DI 10.1088/0067-0049/215/1/13
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS2YH
UT WOS:000344141800013
ER

PT J
AU Heap, SR
   Gong, Q
   Hull, T
   Kruk, J
   Purves, L
AF Heap, Sara R.
   Gong, Qian
   Hull, Tony
   Kruk, Jeffrey
   Purves, Lloyd
TI GESE: a small UV space telescope to conduct a large spectroscopic survey
   of z similar to 1 Galaxies
SO ASTROPHYSICS AND SPACE SCIENCE
LA English
DT Article
DE Galaxy evolution; Ultraviolet; Multi-object spectroscopy; Microshutter
   array; Lightweight mirrors
AB One of the key goals of NASA's astrophysics program is to answer the question: How did galaxies evolve into the spirals and elliptical galaxies that we see today? We describe a space mission concept called Galaxy Evolution Spectroscopic Explorer (GESE) to address this question by making a large spectroscopic survey of galaxies at a redshift, z similar to 1 (look-back time of similar to 8 billion years). GESE is a 1.5-m space telescope with an ultraviolet (UV) multi-object slit spectrograph that can obtain spectra of hundreds of galaxies per exposure. The spectrograph covers the spectral range, 0.2-0.4 mu m at a spectral resolving power, R similar to 500. This observed spectral range corresponds to 0.1-0.2 mu m as emitted by a galaxy at a redshift, z=1. The mission concept takes advantage of two new technological advances: (1) light-weighted, wide-field telescope mirrors, and (2) the Next-Generation MicroShutter Array (NG-MSA) to be used as a slit generator in the multi-object slit spectrograph.
C1 [Heap, Sara R.; Gong, Qian; Kruk, Jeffrey; Purves, Lloyd] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Hull, Tony] Univ New Mexico, Albuquerque, NM 87131 USA.
RP Heap, SR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt Rd, Greenbelt, MD 20771 USA.
EM sally.heap@NASA.gov
NR 8
TC 1
Z9 1
U1 0
U2 2
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 NOV
PY 2014
VL 354
IS 1
BP 211
EP 214
DI 10.1007/s10509-014-1981-0
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS5OW
UT WOS:000344320800028
ER

PT J
AU English, KL
   Loehr, JA
   Lee, SMC
   Smith, SM
AF English, Kirk L.
   Loehr, James A.
   Lee, Stuart M. C.
   Smith, Scott M.
TI Early-phase musculoskeletal adaptations to different levels of eccentric
   resistance after 8 weeks of lower body training
SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE Muscle strength; Hypertrophy; Bone mineral density; Bone formation; Bone
   resorption; Spaceflight; Eccentric overload; Eccentric underload
ID BONE-MINERAL DENSITY; INTERNATIONAL-SPACE-STATION; LONG-DURATION
   SPACEFLIGHT; SKELETAL STRUCTURAL ADAPTATIONS; FLYWHEEL RESISTIVE
   EXERCISE; MECHANICAL USAGE SATMU; CROSS-SECTIONAL AREA; REDEFINING WOLFF
   LAW; HIGH-IMPACT EXERCISE; BED REST
AB Eccentric muscle actions are important to the development of muscle mass and strength and may affect bone mineral density (BMD). This study's purpose was to determine the relative effectiveness of five different eccentric:concentric load ratios to increase musculoskeletal parameters during early adaptations to resistance training.
   Forty male subjects performed a supine leg press and calf press training program 3 days week(-1) for 8 weeks. Subjects were matched for pre-training leg press 1-repetition maximum strength (1-RM) and randomly assigned to one of five training groups. Concentric training load (% 1-RM) was constant across groups, but within groups, eccentric load was 0, 33, 66, 100, or 138 % of concentric load. Muscle mass (dual energy X-ray absorptiometry; DXA), strength (1-RM), and BMD (DXA) were measured pre- and post-training. Markers of bone metabolism were assessed pre-, mid- and post-training.
   The increase in leg press 1-RM in the 138 % group (20 +/- A 4 %) was significantly greater (P < 0.05) than the 0 % (8 +/- A 3 %), 33 % (8 +/- A 5 %) and 66 % (8 +/- A 4 %) groups, but not the 100 % group (13 +/- A 6 %; P = 0.15). All groups, except the 0 % group, increased calf press 1-RM (P < 0.05). Leg lean mass and greater trochanter BMD were increased only in the 138 % group (P < 0.05).
   Early-phase adaptations to eccentric overload training include increases in muscle mass and site-specific increases in BMD and muscle strength which are not present or are less with traditional and eccentric underload training. Eccentric overload provides a robust musculoskeletal stimulus that may benefit bedridden patients, individuals recovering from injury or illness, and astronauts during spaceflight.
C1 [English, Kirk L.] JES Tech LLC, Houston, TX 77058 USA.
   [Loehr, James A.; Lee, Stuart M. C.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
   [Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP English, KL (reprint author), JES Tech LLC, 16870 Royal Crest Dr, Houston, TX 77058 USA.
EM kirk.english-1@nasa.gov
NR 112
TC 3
Z9 3
U1 2
U2 19
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1439-6319
EI 1439-6327
J9 EUR J APPL PHYSIOL
JI Eur. J. Appl. Physiol.
PD NOV
PY 2014
VL 114
IS 11
BP 2263
EP 2280
DI 10.1007/s00421-014-2951-5
PG 18
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA AR9SD
UT WOS:000343915300005
PM 25048074
ER

PT J
AU Asmar, A
   Bulow, J
   Simonsen, L
   Rasmussen, JG
   Christensen, NJ
   Frandsen, E
   Norsk, P
AF Asmar, Ali
   Bulow, Jens
   Simonsen, Lene
   Rasmussen, Jonas G.
   Christensen, Niels J.
   Frandsen, Erik
   Norsk, Peter
TI Circulatory responses to lower body negative pressure in young Afghans
   and Danes: implications for understanding ethnic effects on blood
   pressure regulation
SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE Ethnicity; Orthostatic stress; Cardiac output; Noradrenaline; Renin
ID ORTHOSTATIC TOLERANCE; SYMPATHETIC ACTIVITY; VENOUS DISTENSION; HUMANS;
   HYPOVOLEMIA; TILT; ACTIVATION; STRESS; SYSTEM; VOLUME
AB We have previously shown that Afghans residing in Denmark for at least 12 years exhibit a lower 24-h ambulatory blood pressure compared to Danes. The purpose of this study was to test the hypothesis that the lower blood pressure reflects attenuated compensatory baroreflex responses in the Afghans.
   On a controlled diet (2,822 cal/day, 55-75 mmol + 2 mmol Na+/kg/day), 12 young males of Afghan (Afghans) and 12 young males of Danish (Danes) origin were exposed to a two-step lower body negative pressure (LBNP) protocol of -20 and -50 mmHg, respectively, each of 10-min duration.
   Afghans had lower 24-h systolic blood pressure compared to Danes (115 +/- A 2 vs. 123 +/- A 1 mmHg, p < 0.05). Cardiac output and stroke volume were significantly lower in Afghans compared to Danes prior to and during each level of LBNP. However, it decreased to the same extent in both groups during LBNP. During LBNP of -20 mmHg, plasma noradrenaline concentration and plasma renin activity (PRA) increased significantly only in the Afghans. At LBNP of -50 mmHg plasma noradrenaline concentration and PRA both increased significantly and similarly in the two groups.
   The lower 24-h ambulatory blood pressure in the Afghans is probably caused by a lower stroke volume, which augmented the circulatory and vasoactive hormonal responses to LBNP in the Afghans. The lower stroke volume in Afghans residing in Denmark compared to that of matched native Danes remains to be explained.
C1 [Asmar, Ali; Bulow, Jens; Rasmussen, Jonas G.; Norsk, Peter] Univ Copenhagen, Dept Biomed Sci, Fac Hlth Sci, DK-2200 Copenhagen, Denmark.
   [Asmar, Ali; Bulow, Jens; Simonsen, Lene] Bispebjerg Hosp, Dept Clin Physiol & Nucl Med, DK-2400 Copenhagen, Denmark.
   [Christensen, Niels J.] Herlev Univ Hosp, Dept Internal Med & Endocrinol, DK-2730 Herlev, Denmark.
   [Frandsen, Erik] Glostrup Univ Hosp, Dept Diagnost Clin Physiol & Nucl Med, DK-2600 Glostrup, Denmark.
   [Norsk, Peter] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
   [Norsk, Peter] NASA, Biomed Res & Environm Sci Div, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Asmar, A (reprint author), Bispebjerg Hosp, Dept Clin Physiol & Nucl Med, DK-2400 Copenhagen, Denmark.
EM aliasmar@sund.ku.dk
FU Danish Research Councils (Danish Agency for Science, Technology and
   Innovation) [272-07-0614]
FX The efficient support of our laboratory technician, Jakob Utzon-Frank is
   gratefully acknowledged. This study was supported by Grant No.
   272-07-0614 from the Danish Research Councils (Danish Agency for
   Science, Technology and Innovation).
NR 30
TC 0
Z9 0
U1 2
U2 5
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1439-6319
EI 1439-6327
J9 EUR J APPL PHYSIOL
JI Eur. J. Appl. Physiol.
PD NOV
PY 2014
VL 114
IS 11
BP 2321
EP 2329
DI 10.1007/s00421-014-2946-2
PG 9
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA AR9SD
UT WOS:000343915300010
PM 25059759
ER

PT J
AU Spak, K
   Agnes, G
   Inman, D
AF Spak, K.
   Agnes, G.
   Inman, D.
TI Parameters for Modeling Stranded Cables as Structural Beams
SO EXPERIMENTAL MECHANICS
LA English
DT Article
DE Cable properties; Wire modeling; Cable bending stiffness; Cable
   constraints; Cable resonance
ID EXPERIMENTAL VALIDATION; WIRE STRANDS; CONDUCTORS
AB This paper presents a method for determining the effective homogenous beam parameters for stranded cables made up of non-homogenous wires, as well as characterization of the attachment method commonly used for cable harnesses on space structures. There is not yet a predictive model for quantifying the structural impact of cable harnesses on space flight structures, and towards this goal, the authors aim to predict cable resonance behavior from basic cable measurements. Cables can be modeled as shear beams, but the shear beam model assumes a homogenous, isotropic material, which a stranded cable is not. Thus, the cable-beam model requires both knowledge of the cable constraints and calculation of effectively homogenous properties, including density, area, bending stiffness, and modulus of rigidity to predict the natural frequencies of the cable. Through a combination of measurement and correction factors, upper and lower bounds for effective cable properties and attachment stiffness are calculated and shown to be effective in a cable-beam model for natural frequency prediction. Although the cables investigated are spaceflight cables, the method can be applied to any stranded cable for which the constituent material properties can be determined.
C1 [Spak, K.] Virginia Tech, Blacksburg, VA USA.
   [Agnes, G.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Inman, D.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA.
RP Spak, K (reprint author), 916 Oak Ave, Redwood City, CA 94061 USA.
EM kspak@vt.edu; greg.s.agnes@jpl.nasa.gov; daninman@umich.edu
FU NASA Office of the Chief Technologist's Space Technology Research
   Fellowship; AFOSR [FA9550-10-1-0427]
FX This work was supported by a NASA Office of the Chief Technologist's
   Space Technology Research Fellowship. Cables for experimental validation
   were provided at cost by Southern California Braiding Company. The third
   author gratefully acknowledges the support of AFOSR Grant number
   FA9550-10-1-0427 monitored by Dr. David Stargel. 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 20
TC 4
Z9 4
U1 1
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0014-4851
EI 1741-2765
J9 EXP MECH
JI Exp. Mech.
PD NOV
PY 2014
VL 54
IS 9
BP 1613
EP 1626
DI 10.1007/s11340-014-9941-8
PG 14
WC Materials Science, Multidisciplinary; Mechanics; Materials Science,
   Characterization & Testing
SC Materials Science; Mechanics
GA AS3BC
UT WOS:000344149800010
ER

PT J
AU Malaska, MJ
   Hodyss, R
AF Malaska, Michael J.
   Hodyss, Robert
TI Dissolution of benzene, naphthalene, and biphenyl in a simulated Titan
   lake
SO ICARUS
LA English
DT Article
DE Titan; Geological processes; Titan, hydrology; Titan, surface
ID CHEMICAL-COMPOSITION; ONTARIO LACUS; HUYGENS PROBE; CASSINI VIMS;
   LANDING SITE; SURFACE; ATMOSPHERE; LIQUID; METHANE; UNCERTAINTIES
AB We constructed a laboratory apparatus capable of measuring the saturation equilibrium concentration (c(sat)) and dissolution rate constants (k(eff)) of organic solutes in ethane at 94 K. We determined a c(sat) of 18.5 +/- 1.9 mg L-1, 0.159 +/- 0.003 mg L-1, and 0.039 +/- 0.006 mg L-1 for benzene, naphthalene, and biphenyl, respectively. The derived c(sat) and k(eff) can be used to predict the dissolution behavior of the materials in ethane under Titan conditions. The aromatic materials dissolved relatively quickly in liquid ethane at 94 K, reaching saturation in less than 2 h. The dissolution characteristics of benzene in ethane at 94 K are compared to those of terrestrial karst-forming materials in water at 298 K, and are used to constrain Titan surface processes. We discuss the implications of our measurements on the formation of karst on Titan, the concentration of organics in Titan's lakes, and the formation of evaporite deposits during lake evaporation. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Malaska, Michael J.; Hodyss, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Malaska, MJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM MichaelJ.Malaska@jpl.nasa.gov; Robert.P.Hodyss@jpl.nasa.gov
OI Malaska, Michael/0000-0003-0064-5258
FU NASA Postdoctoral Program at the Jet Propulsion Laboratory; NASA Outer
   Planets Research (OPR) program; NASA Astrobiology Institute (Titan);
   NASA's Astrobiology Science and Technology Instrument Development
   (ASTID) program; NASA; Government sponsorship
FX The authors would like to thank V.F. Chevrier and an anonymous reviewer
   for constructive suggestions to this manuscript. This research was
   supported by an appointment to the NASA Postdoctoral Program at the Jet
   Propulsion Laboratory, administered by Oak Ridge Associated Universities
   through a contract with NASA as well as a grant from the NASA Outer
   Planets Research (OPR) program. Support from the NASA Astrobiology
   Institute (Titan) and NASA's Astrobiology Science and Technology
   Instrument Development (ASTID) program is gratefully acknowledged. This
   work was carried out at the Jet Propulsion Laboratory, California
   Institute of Technology, under contract with NASA. Copyright 2014,
   California Institute of Technology. Government sponsorship is
   acknowledged.
NR 68
TC 12
Z9 12
U1 2
U2 19
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD NOV 1
PY 2014
VL 242
BP 74
EP 81
DI 10.1016/j.icarus.2014.07.022
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS0KX
UT WOS:000343967100007
ER

PT J
AU Boxe, CS
   Francisco, JS
   Shia, RL
   Yung, YL
   Nair, H
   Liang, MC
   Saiz-Lopez, A
AF Boxe, C. S.
   Francisco, J. S.
   Shia, R. -L.
   Yung, Y. L.
   Nair, H.
   Liang, M. -C.
   Saiz-Lopez, A.
TI New insights into martian atmospheric chemistry
SO ICARUS
LA English
DT Article
DE Mars; Atmospheres, chemistry; Atmospheres, composition
ID TRANS-HOCO; DISSOCIATIVE PHOTODETACHMENT; PRESSURE-DEPENDENCE; MARS
   ATMOSPHERE; CO; SPECTROSCOPY; TEMPERATURE; STABILITY; OH; PHOTOCHEMISTRY
AB HOx radicals are produced in the martian atmosphere by the photolysis of water vapor and subsequently participate in catalytic cycles that recycle carbon dioxide (CO2) from its photolysis product carbon monoxide (CO), providing a qualitative explanation for the stability of its atmosphere. Balancing CO2 production and loss based on our current understanding of martian gas-phase chemistry has, however, proven to be difficult. The photolysis of O-3 produces O(D-1), while oxidation of CO produces HOCO radicals, a new member of the HOx family. The O(D-1) quantum yield has recently been updated, which quantifies non-zero quantum yields in the Huggins bands. In Earth's atmosphere HOCO is considered to be unimportant since it is quickly removed by abundant oxygen molecules. The smaller amount of O-2 in the Mars' atmosphere causes HOCO's lifetime to be longer in Mars' atmosphere than Earth's (3 x 10(-5) s to 1.2 days from Mars's surface to 240 km, respectively). Limited kinetic data on reactions involving HOCO prevented consideration of its reactions directly in atmospheric models. Therefore, the impact of HOCO reactions on martian chemistry is currently unknown. Here, we incorporate new literature rate constants for HOCO chemistry and an updated representation of the O(D-1) quantum yield in the Caltech/JPL 1-D photochemical model for Mars' atmosphere. Our simulations exemplify perturbations to NOy, HOx and COx species, ranging from 5% to 50%. The modified O(D-1) quantum yield and new HOCO chemistry cause a 10% decrease and a 50% increase in OH and H2O2 total column abundances, respectively. At low altitudes, HOCO production contributes 5% towards CO2 production. Given recent experimentally-obtained branching ratios for the oxidation of CO, HOCO may contribute up to 70% toward the production of NOy, where HOx and NOy species are enhanced up to a factor 3, which has implications for rethinking the fundamental understanding of NOy, HOx, and CO/CO2 cycling on Mars. Two new reaction mechanisms for converting CO to CO2 using HOCO reactions are proposed, which reveal that H2O2 is more intimately coupled to COx chemistry. Our simulations are in good agreement with satellite/spacecraft measurements of CO and H2O2 on Mars. Published by Elsevier Inc.
C1 [Boxe, C. S.] CALTECH, Jet Prop Lab, NASA, Earth & Space Sci Div, Pasadena, CA 91109 USA.
   [Boxe, C. S.] CUNY Medgar Evers Coll, Brooklyn, NY 11225 USA.
   [Boxe, C. S.] CUNY, Grad Ctr, Div Chem, New York, NY 10016 USA.
   [Boxe, C. S.] CUNY, Grad Ctr, Earth & Environm Sci Div, New York, NY 10016 USA.
   [Francisco, J. S.] Purdue Univ, Dept Chem & Earth & Atmospher Sci, W Lafayette, IN 47907 USA.
   [Shia, R. -L.; Yung, Y. L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
   [Nair, H.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20273 USA.
   [Liang, M. -C.] Natl Cent Univ, Acad Sinica, Res Ctr Environm Studies, Inst Astron, Taipei, Taiwan.
   [Liang, M. -C.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
   [Saiz-Lopez, A.] CSIC, Inst Phys Chem Rocasolano, Atmospher Chem & Climate Grp, Madrid, Spain.
RP Boxe, CS (reprint author), CUNY Medgar Evers Coll, Brooklyn, NY 11225 USA.
EM boxeman3@gmail.com
RI Saiz-Lopez, Alfonso/B-3759-2015
OI Saiz-Lopez, Alfonso/0000-0002-0060-1581
NR 39
TC 2
Z9 2
U1 7
U2 32
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 NOV 1
PY 2014
VL 242
BP 97
EP 104
DI 10.1016/j.icarus.2014.07.023
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS0KX
UT WOS:000343967100009
ER

PT J
AU Trammell, HJ
   Li, LM
   Jiang, X
   Smith, M
   Horst, S
   Vasavada, A
AF Trammell, Harold Justin
   Li, Liming
   Jiang, Xun
   Smith, Mark
   Hoerst, Sarah
   Vasavada, Ashwin
TI The global vortex analysis of Jupiter and Saturn based on Cassini
   Imaging Science Subsystem
SO ICARUS
LA English
DT Article
DE Saturn, atmosphere; Atmospheres, dynamics; Atmospheres, structure; Image
   processing
ID MOIST CONVECTION; EQUATORIAL JET; CLOUD LEVEL; ATMOSPHERE; DYNAMICS;
   VORTICES; EDDIES; IMAGES; WINDS; MORPHOLOGY
AB Presented in this manuscript are observations exploring vortices with diameters larger than 1000 km on Jupiter and Saturn. These images are taken from the Imaging Science Subsystem onboard the Cassini Spacecraft. The analyses of Saturn's vortices show that there are significantly more vortices in the Southern Hemisphere (SH) than in the Northern Hemisphere (NH) during the time from 2004 to 2010. In particular, the concentration of vortices are completely different between the two hemispheres, especially in the latitude band around 40 degrees N where the 2010 giant storm occurred. In the SH, the latitude band around 40 degrees S has the highest concentration of vortices on Saturn. Contrasting results show that vortices are lacking in the latitudinal band around 40 degrees N in the NH before the eruption of the 2010 giant storm, although zonal wind characteristics are similar at both locations. Global maps of Saturn at different times suggest that the total numbers of large vortices dramatically decreased from 29 +/- 1 to 11 +/- 2 in the SH and from 11 +/- 2 to 7 +/- 1 in the NH during this time period (2004-2010), just before the eruption of the giant storm at the end of 2010. The goal here is to present observational trends and evaluate if the temporal variation in the total number of vortices is related to the eruption of the 2010 giant storm. The comparison of jovian and saturnian vortices shows that the contrast of the two hemispheres is different between the two giant planets, likely due to the different obliquities, hence different seasonal cycles on the two planets. Jovian vortices tend to display a near equal distribution of vortices across hemispheres, while saturnian vortices are distributed unevenly. The comparison also reveals that on both planets, there is a correlation between the highest number of vortices and the westward jet peaks. This suggests that atmospheric instabilities play a critical role in generating vortices on both planets. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Trammell, Harold Justin; Li, Liming; Jiang, Xun; Smith, Mark] Univ Houston, Houston, TX 77020 USA.
   [Hoerst, Sarah] Univ Colorado, Boulder, CO 80309 USA.
   [Vasavada, Ashwin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Trammell, HJ (reprint author), Univ Houston, 4800 Calhoun Rd, Houston, TX 77020 USA.
EM hjtrammell@uh.edu
RI Horst, Sarah/A-9906-2010
OI Horst, Sarah/0000-0003-4596-0702
FU NASA Cassini Data Analysis Program; Outer Planets Research Program; NSF
   Astronomy and Astrophysics Postdoctoral Fellowship [AST-1102827]
FX NASA Cassini Data Analysis and Outer Planets Research Programs funded
   this work. We also acknowledge the Cassini ISS team for providing the
   multi-filter images of Jupiter and Saturn. S.M.H. is supported by NSF
   Astronomy and Astrophysics Postdoctoral Fellowship AST-1102827.
NR 38
TC 3
Z9 3
U1 3
U2 11
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 NOV 1
PY 2014
VL 242
BP 122
EP 129
DI 10.1016/j.icarus.2014.07.019
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS0KX
UT WOS:000343967100012
ER

PT J
AU Rodriguez, JAP
   Gulick, VC
   Baker, VR
   Platz, T
   Fairen, AG
   Miyamoto, H
   Kargel, JS
   Rice, JW
   Glines, N
AF Rodriguez, J. Alexis P.
   Gulick, Virginia C.
   Baker, Victor R.
   Platz, Thomas
   Fairen, Alberto G.
   Miyamoto, Hideaki
   Kargel, Jeffrey S.
   Rice, James W.
   Glines, Natalie
TI Evidence for Middle Amazonian catastrophic flooding and glaciation on
   Mars
SO ICARUS
LA English
DT Article
DE Mars; Surface; Geological processes
ID OUTFLOW CHANNELS; VALLES-MARINERIS; GRAVEL DUNES; ICE; FLOWS; EVOLUTION;
   SURFACE; ORIGIN; CHAOS; WATER
AB Early geologic investigations of Mars revealed some of the largest channels in the Solar System (outflow channels), which appear to have mostly developed similar to 3 byr ago. These channels have been the subject of much scientific inquiry since the 1970s and proposed formative processes included surface erosion by catastrophic floods, glaciers, debris flows and lava flows. Based on the analysis of newly acquired Mars Reconnaissance Orbiter (MRO) Context (CTX, 5.15-5.91 m/pixel) and High Resolution Imaging Science Experiment (HiRISE, 25-50 cm/pixel) image data, we have identified a few locations contained within relatively narrow canyons of the southern circum-Chryse outflow channels that retain well-preserved decameter/hectometer-scale landform assemblages. These terrains include landforms consistent in shape, dimension and overall assemblage to those produced by catastrophic floods, and at one location, to glacial morphologies. Impact crater statistics for four of these surfaces, located within upstream, midstream and downstream outflow channel surfaces, yield an age estimate of similar to 600 myr. This suggests that the southern circum-Chryse outflow channels were locally resurfaced by some of the most recent catastrophic floods on the planet, and that these floods coexisted within regional glacier environments as recently as during the Middle Amazonian. (C) 2014 Published by Elsevier Inc.
C1 [Rodriguez, J. Alexis P.; Gulick, Virginia C.; Glines, Natalie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Rodriguez, J. Alexis P.; Platz, Thomas; Rice, James W.] Planetary Sci Inst, Tucson, AZ 85719 USA.
   [Gulick, Virginia C.] SETI Inst, Mountain View, CA 94043 USA.
   [Baker, Victor R.; Kargel, Jeffrey S.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA.
   [Platz, Thomas] Free Univ Berlin, Inst Geol Sci, D-12249 Berlin, Germany.
   [Fairen, Alberto G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
   [Miyamoto, Hideaki] Univ Tokyo, Univ Museum, Tokyo 1130033, Japan.
RP Rodriguez, JAP (reprint author), NASA, Ames Res Ctr, Mail Stop 239-20, Moffett Field, CA 94035 USA.
EM Alexis.Rodriguez@NASA.gov
RI Platz, Thomas/F-7539-2013; Miyamoto, Hideaki/B-9666-2008
OI Platz, Thomas/0000-0002-1253-2034; 
FU NASA's NPP program; MRO HiRISE Co-Investigator funds; DFG [PL61312-1];
   KAKENHI [23340126]
FX 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 (PL61312-1) and the Helmholtz association through the
   research alliance "Planetary Evolution and Life". 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 53
TC 5
Z9 5
U1 3
U2 19
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD NOV 1
PY 2014
VL 242
BP 202
EP 210
DI 10.1016/j.icarus.2014.06.008
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS0KX
UT WOS:000343967100020
ER

PT J
AU Hardersen, PS
   Reddy, V
   Roberts, R
   Mainzer, A
AF Hardersen, Paul S.
   Reddy, Vishnu
   Roberts, Rachel
   Mainzer, Amy
TI More chips off of Asteroid (4) Vesta: Characterization of eight Vestoids
   and their HED meteorite analogs
SO ICARUS
LA English
DT Article
DE Asteroids; Asteroids, composition; Mineralogy; Spectroscopy
ID V-TYPE ASTEROIDS; OUTER MAIN BELT; NEAR-EARTH ASTEROIDS; SPECTROSCOPIC
   SURVEY; REFLECTANCE SPECTRA; DAWN MISSION; MU-M; MINERALOGICAL
   CHARACTERIZATION; BASALTIC ASTEROIDS; SOLAR-SYSTEM
AB Vestoids are generally considered to be fragments from Asteroid (4) Vesta that were ejected by past collisions that document Vesta's collisional history. Dynamical Vestoids are defined by their spatial proximity with Vesta (Zappala, V., Bendjoya, Ph., Cellino, A., Farinella, P., Froeschle', C. [1995]. Icarus 116, 291-314; Nesvorny, D. [2012]. Nesvorny HCM Asteroid Families V2.0. EAR-A-VARGBDET-5-NESV-ORNYFAM-V2.0. NASA Planetary Data System.). Taxonomic Vestoids are defined as V-type asteroids that have a photometric, visible-wavelength spectral, or other observational relationship with Vesta (Tholen, DJ., 1984. Asteroid Taxonomy from Cluster Analysis of Photometry. Ph.D. Thesis, University of Arizona, Tucson; Bus, S.J., Binzel, R.P. [2002]. Icarus 158, 106-145; Carvano, J., Hasselmann, P.H., Lazzaro, D., Mothe'-Diniz, T. [2010]. Astron. Astrophys. 510, A43). We define 'genetic Vestoids' as V-type asteroids that are probable fragments ejected from (4) Vesta based on the supporting combination of dynamical, near-infrared (NIR) spectral, and taxonomic evidence. NIR reflectance spectroscopy is one of the primary ground-based techniques to constrain an asteroid's major surface mineralogy (Burns, R.G. [1993a]. Mineralogical Applications of Crystal Field Theory. Cambridge University Press, Cambridge, UK, 551 p). Despite the reasonable likelihood that many dynamical and taxonomic Vestoids likely originate from Vesta, ambiguity exists concerning the fraction of these populations that are from Vesta as compared to the fraction of asteroids that might not be related to Vesta.
   Currently, one of the most robust techniques to identify the genetic Vestoid population is through NIR reflectance spectroscopy from similar to 0.7 to 2.5 mu m. The derivation of spectral band parameters, and the comparison of those band parameters with those from representative samples from the Howardite-Eucrite-Diogenite (HED) meteorite types, allows a direct comparison of their primary mineralogies. Establishing tighter constraints on the genetic Vestoid population will better inform mass estimates for the current population of probable Vestoids, will provide more accurate orbital information of Vestoid migration through time that will assist dynamical models, and will constrain the overall current abundance of basaltic material in the main asteroid belt (Moskovitz, N.A., Jedicke, R., Gaidos, E., Willman, M., Nesvorny, D., Fevig, R. [2008]. Icarus 198, 77-90).
   This work reports high-quality NIR spectra, and their respective interpretations, for eight V5-type asteroids, as defined by Carvano et al. (Carvano, J., Hasselmann, P.H., Lazzaro, D., Mothe'-Diniz, T. [2010]. Astron. Astrophys. 510, A43), that were observed at the NASA Infrared Telescope Facility on January 14, 2013 UT. They include: (3867) Shiretoko, (5235) Jean-Loup, (5560) Amytis, (6331) 1992 FZ1, (6976) Kanatsu, (17469) 1991 BT, (29796) 1999 CW77, and (30872) 1992 EM17. All eight asteroids exhibit the broad similar to 0.9- and similar to 1.9-mu m mineral absorption features indicative of pyroxene on each asteroid's surface. Data reduction and analysis via multiple techniques produced consistent results for the derived spectral absorption band centers and average pyroxene surface chemistries for all eight asteroids (Reddy, V., Sanchez, J.A., Nathues, A., Moskovitz, N.A., Li, J.-Y, Cloutis, E.A., Archer, K., Tucker, R.A., Gaffey, M.J., Mann, P.J., Sierks, H., Schade, U. [2012c]. Icarus 217, 153-168; Lindsay, S.S., Emery, J.P., Marchis, F., Enriquez, J., Assafin, M. [2013]. A spectroscopic and mineralogic study of multiple asteroid systems. American Astronomical Society, DPS Meeting #45, #112.04; Lindsay, S.S., Marchis, F., Emery, J.P., Enriquez, J.E., Assafin, M. [2014]. Icarus, submitted for publication; Gaffey, M.J., Cloutis, E.A., Kelley, M.K., Reed, K.L. [2002]. Mineralogy of asteroids. In: Bottke Jr., W.F., Cellino, A., Paolicchi, P., Binzel, R.P. (Eds.), Asteroids III. The University of Arizona Press, Tucson, pp. 183-204; Burbine, T.H., Buchanan, P.C., Dolkar, T., Binzel, R.P. [2009]. Met. Planet. Sci. 44,1331-1341.). (3867) Shiretoko is most consistent with the eucrite meteorites while the remaining seven asteroids are most consistent with the howardite meteorites. The existing evidence suggests that all eight of these V-p-type asteroids are genetic Vestoids that probably originated from Vesta's surface. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Hardersen, Paul S.; Roberts, Rachel] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
   [Reddy, Vishnu] Planetary Sci Inst, Tucson, AZ 85719 USA.
   [Mainzer, Amy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hardersen, PS (reprint author), Univ N Dakota, Dept Space Studies, 4149 Univ Ave,Stop 9008,530 Clifford Hall, Grand Forks, ND 58202 USA.
EM Hardersen@space.edu; reddy@psi.edu; momenttensor@gmail.com;
   amy.mainzer@jpl.nasa.gov
OI Reddy, Vishnu/0000-0002-7743-3491
FU NASA Planetary Astronomy Program [NNX14AJ37G]; National Aeronautics and
   Space Administration
FX This work is supported by NASA Planetary Astronomy Program Grant
   #NNX14AJ37G. This publication makes use of data products from the
   Wide-Field Infrared Survey Explorer, which is a joint project of the
   University of California, Los Angeles, and the Jet Propulsion
   Laboratory/California Institute of Technology, funded by the National
   Aeronautics and Space Administration.
NR 121
TC 4
Z9 4
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 NOV 1
PY 2014
VL 242
BP 269
EP 282
DI 10.1016/j.icarus.2014.08.020
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS0KX
UT WOS:000343967100024
ER

PT J
AU de Kleer, K
   de Pater, I
   Davies, AG
   Adamkovics, M
AF de Kleer, Katherine
   de Pater, Imke
   Davies, Ashley Gerard
   Adamkovics, Mate
TI Near-infrared monitoring of Io and detection of a violent outburst on 29
   August 2013
SO ICARUS
LA English
DT Article
DE Io; Volcanism; Infrared observations
ID GROUND-BASED OBSERVATIONS; JUPITERS MOON IO; VOLCANIC ACTIVITY; GALILEO
   NIMS; HEAT-FLOW; TEMPERATURE; SPECTROGRAPH; MISSION; IMAGER; LAKES
AB We present initial data from our campaign to monitor Jo in the near-infrared, beginning in August 2013, using 3.8-mu m adaptive optics imaging at Gemini N and 2-5 mu m disk-integrated spectroscopy at NASA's IRTF. Conducted during 2013-2014, these observations are coincident with the ISAS/JAXA EXCEED mission's continuous monitoring of the Jo plasma torus and will enable the speculated effects of volcanic outgassing on the torus to be observed directly, in addition to enabling an assessment of the frequency and properties of large-scale outbursts. On 29 August 2013 we detected a powerful eruption (designated 201308C) on Jo at 223.5 +/- 2.6 degrees W, 29.1 +/- 1.8 degrees N. Emitting between 15 and >25 TW, this event is one of the most powerful eruptions ever seen on Io and falls into the rare "outburst" class. This was the third eruption of this type seen on Io in August 2013, an unprecedented occurrence. Also unprecedented was the charting of the decay in thermal emission over the subsequent days and weeks. Modeling of the outburst spectrum places a lower bound of 1200-1300 K on the eruption temperature, and is suggestive of temperatures 1900 K or higher, typically associated with ultramafic lava composition. The eruption is likely a highly energetic, high-volume lava fountain event. (C) 2014 Elsevier Inc. All rights reserved.
C1 [de Kleer, Katherine; de Pater, Imke; Adamkovics, Mate] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [de Pater, Imke] Delft Univ Technol, Delft Inst Earth Observat & Space Syst, NL-2629 HS Delft, Netherlands.
   [de Pater, Imke] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
   [Davies, Ashley Gerard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP de Kleer, K (reprint author), Univ Calif Berkeley, Dept Astron, B-20 Hearst Field Annex, Berkeley, CA 94720 USA.
EM kdekleer@berkeley.edu
FU Gemini N Telescope [GN-2013B-DD-3]; Visiting Astronomer at NASA's
   Infrared Telescope Facility [2013B-030]; National Science Foundation,
   NSF [AST-1313485]; National Science Foundation [DGE-1106400]; NASA Outer
   Planets Research
FX The data presented in this paper were obtained at the Gemini N Telescope
   and as a Visiting Astronomer at NASA's Infrared Telescope Facility,
   under programs GN-2013B-DD-3 and 2013B-030 respectively. We thank the
   Gemini Director, Markus Kissler-Patig, and the Deputy Director and Head
   of Science, Nancy Levenson, for providing us with DD time to observe Io
   during about a dozen nights following the initial detection of the
   eruption. We thank the IRTF Director, Alan Tokunaga, for providing us
   with DD time to simultaneously observe Io on four of these nights.
   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). The Infrared Telescope
   Facility is operated by the University of Hawaii under Cooperative
   Agreement No. NNX-08AE38A with the National Aeronautics and Space
   Administration, Science Mission Directorate, Planetary Astronomy
   Program. Our research was partially supported by the National Science
   Foundation, NSF Grant AST-1313485 to UC Berkeley, and by the National
   Science Foundation Graduate Research Fellowship under Grant DGE-1106400.
   Ashley Davies thanks the NASA Outer Planets Research and Planetary
   Geology and Geophysics Programs for support. The authors recognize and
   acknowledge the very significant cultural role and reverence that the
   summit of Mauna Kea has always had within the indigenous Hawaiian
   community. We are most fortunate to have the opportunity to conduct
   observations of Ionian volcanoes from this Hawaiian volcano.
NR 48
TC 11
Z9 11
U1 0
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD NOV 1
PY 2014
VL 242
BP 352
EP 364
DI 10.1016/j.icarus.2014.06.006
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS0KX
UT WOS:000343967100029
ER

PT J
AU de Pater, I
   Davies, AG
   Adamkovics, M
   Ciardi, DR
AF de Pater, Imke
   Davies, Ashley Gerard
   Adamkovics, Mate
   Ciardi, David R.
TI Two new, rare, high-effusion outburst eruptions at Rarog and Heno
   Paterae on Io
SO ICARUS
LA English
DT Article
DE Io; Volcanism; Infrared observations
ID GROUND-BASED OBSERVATIONS; JUPITERS MOON IO; HEAT-FLOW;
   VOLCANIC-ERUPTIONS; THERMAL SIGNATURE; GALILEO; TEMPERATURES;
   INSTRUMENT; TELESCOPE; EVOLUTION
AB Observations obtained with the near-infrared camera NIRC2, coupled to the adaptive optics system on the 10-m W.M. Keck II telescope on Mauna Kea, Hawaii, on 15 August 2013 at similar to 15:30 UT revealed two large "Outburst"-class volcanic eruptions on Io. Follow-up observations five days later showed that both eruptions had substantially faded. The most energetic eruption was at Rarog Patera, at a location near 305 degrees W, 42 degrees S; a smaller one occurred further south at similar to 310 degrees W and similar to 57 degrees S, close to Heno Patera. Total radiant fluxes at Rarog Patera on August 15 were of order similar to 500 GW/sr/mu m at wavelengths between 2 and 4 p,m, and close to 250 GW/sr/mu m at 1.6 mu m, indicative of an effective temperature of similar to 1040 K over an area of similar to 120 km(2), and a total thermal emission of nearly 8 TW. At Heno Patera the 4-mu m flux measured similar to 250 GW/sr/mu m, and similar to 90 GW/sr/mu m at 2.2 mu m, suggestive of an effective temperature of similar to 720 K over an area of more than 300 km(2), and a total thermal emission of similar to 5-6 TW. Fits of the Davies (Davies, AG. [1996]. Icarus 124(1), 45-61) Io Flow Model indicate that these two eruptions are vigorous and the exposed surfaces are mostly very young, no older than 4-5 min at Rarog Patera and a few hours at Heno Patera. The model fits suggest that in both locations lava fountaining is taking place, a highly-energetic style of volcanism. Using follow-up observations taken between August 20 and September 7 we estimate peak effusion rates between 5 x 10(4) and 10(5) m(3)/s. (C) 2014 Elsevier Inc. All rights reserved.
C1 [de Pater, Imke; Adamkovics, Mate] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [de Pater, Imke] Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands.
   [de Pater, Imke] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
   [Davies, Ashley Gerard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP de Pater, I (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM imke@berkeley.edu
OI Ciardi, David/0000-0002-5741-3047
FU W.M. Keck Foundation; National Science Foundation, NSF [AST-1313485];
   NASA Outer Planets Research
FX The Keck Telescopes are 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 Gemini Observatory provides the astronomical communities in each
   partner country with state-ofthe-art astronomical facilities that
   allocate observing time in proportion to each country's contribution.
   The observatory is operated by the Association of Universities for
   Research in Astronomy, Inc., under a cooperative agreement with the NSF
   on behalf of the Gemini partnership: the National Science Foundation
   (United States), the Science and Technology Facilities Council (United
   Kingdom), the National Research Council (Canada), CONICYT (Chile), the
   Australian Research Council (Australia), Ministerio da Ciencia e
   Tecnologia (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion
   Productiva (Argentina). Our research was partially supported by the
   National Science Foundation, NSF Grant AST-1313485 to UC Berkeley.
   Ashley Davies thanks the NASA Outer Planets Research and Planetary
   Geology and Geophysics Program for support. The authors recognize and
   acknowledge the very significant cultural role and reverence that the
   summit of Mauna Kea has always had within the indigenous Hav iaiian
   community. We are most fortunate to have the opportunity to conduct
   observations of Ionian volcanoes from this Hawaiian volcano.
NR 51
TC 9
Z9 9
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 NOV 1
PY 2014
VL 242
BP 365
EP 378
DI 10.1016/j.icarus.2014.06.016
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS0KX
UT WOS:000343967100030
ER

PT J
AU de Pater, I
   Davies, AG
   McGregor, A
   Trujillo, C
   Adamkovics, M
   Veeder, GJ
   Matson, DL
   Leone, G
AF de Pater, Imke
   Davies, Ashley Gerard
   McGregor, Alistair
   Trujillo, Chad
   Adamkovics, Mate
   Veeder, Glenn J.
   Matson, Dennis L.
   Leone, Giovanni
CA Gemini Io Team
TI Global near-IR maps from Gemini-N and Keck in 2010, with a special focus
   on Janus Patera and Kanehekili Fluctus
SO ICARUS
LA English
DT Article
DE Io; volcanism; Infrared observations
ID STANDARD STARS; HEAT-FLOW; THERMAL EMISSION; VOLCANIC ACTIVITY; ACTIVE
   VOLCANISM; LAVA LAKES; IO; GALILEO; ERUPTION; SYSTEM
AB We have imaged Io in the near-infrared (1-5 mu m) with adaptive optics on the 10-m W.M. Keck II and the Gemini North telescopes. We have constructed global maps from the data taken in 2010. Although numerous hot spots are visible, the maps are dominated by two volcanic centers: Loki Patera and Kanehekili Fluctus.
   We have examined in detail the thermal emission from Janus Patera and Kanehekili Fluctus using images obtained between 2003 and 2010, and have created a timeline of volcanic activity at these locations utilizing data from a wide variety of sources. Based on our data and this timeline we find that the thermal emission from Janus Patera is relatively steady, indicative of an active lava lake. The thermal emission from Kanehekili Fluctus, however, is quite variable, and is indicative of the emplacement of extensive lava flows. In 2010, the thermal emission from this location was similar to 10 times higher than ever seen before, indicative of a particularly voluminous eruption of lava. (C) 2014 Elsevier Inc. All rights reserved.
C1 [de Pater, Imke; McGregor, Alistair; Adamkovics, Mate] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [de Pater, Imke] Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands.
   [de Pater, Imke] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
   [Davies, Ashley Gerard; Matson, Dennis L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Trujillo, Chad] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA.
   [Veeder, Glenn J.] Bear Fight Inst, Winthrop, WA 98862 USA.
   [Leone, Giovanni] ETH, Inst Geophys, CH-8092 Zurich, Switzerland.
RP de Pater, I (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM imke@berkeley.edu
RI Lopes, Rosaly/D-1608-2016
OI Leone, Giovanni/0000-0003-1479-9039; Lopes, Rosaly/0000-0002-7928-3167
FU W.M. Keck Foundation; National Science Foundation (United States);
   National Research Council (Canada); CONICYT (Chile); Australian Research
   Council (Australia); Ministerio da Ciencia, Tecnologia e Inovacao
   (Brazil); Ministerio de Ciencia, Tecnologia e Innovacion Productiva
   (Argentina); National Science Foundation, NSF [AST-1313485]; NASA Outer
   Planets Research and Planetary Geology and Geophysics Program
FX The data presented in this paper were obtained at the W.M. Keck and
   Gemini North Observatories. The Keck Telescopes are 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 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). The program ID was GN-2010B-Q-83. Our research
   was partially supported by the National Science Foundation, NSF Grant
   AST-1313485 to UC Berkeley. Ashley Davies thanks the NASA Outer Planets
   Research and Planetary Geology and Geophysics Program for support. The
   authors recognize and acknowledge the very significant cultural role and
   reverence that the summit of Mauna Kea has always had within the
   indigenous Hawaiian community: We are most fortunate to have the
   opportunity to conduct observations of Ionian volcanoes from this
   Hawaiian volcano. We thank the Gemini Io Team: Franck Marchis (SETI),
   Heidi Hammel (AURA), David Williams (ASU), Mike Wong (UCB), John Spencer
   (SWRI), Rosaly Lopes (JPL), and Bert Vermeersen (TUD), among others.
NR 60
TC 7
Z9 7
U1 0
U2 0
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 NOV 1
PY 2014
VL 242
BP 379
EP 395
DI 10.1016/j.icarus.2014.06.019
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS0KX
UT WOS:000343967100031
ER

PT J
AU Cecotti, H
   Eckstein, MP
   Giesbrecht, B
AF Cecotti, Hubert
   Eckstein, Miguel P.
   Giesbrecht, Barry
TI Single-Trial Classification of Event-Related Potentials in Rapid Serial
   Visual Presentation Tasks Using Supervised Spatial Filtering
SO IEEE TRANSACTIONS ON NEURAL NETWORKS AND LEARNING SYSTEMS
LA English
DT Article
DE Brain-computer interface (BCI); common spatial patterns (CSP);
   convolution; electroencephalogram (EEG); neural networks; rapid serial
   visual presentation (RSVP); spatial filters
ID BRAIN-COMPUTER INTERFACE; P300 AMPLITUDE; IMAGE SEARCH; EEG; MODEL;
   TIME; RECOGNITION; RESPONSES; VISION; BCI
AB Accurate detection of single-trial event-related potentials (ERPs) in the electroencephalogram (EEG) is a difficult problem that requires efficient signal processing and machine learning techniques. Supervised spatial filtering methods that enhance the discriminative information in EEG data are commonly used to improve single-trial ERP detection. We propose a convolutional neural network (CNN) with a layer dedicated to spatial filtering for the detection of ERPs and with training based on the maximization of the area under the receiver operating characteristic curve (AUC). The CNN is compared with three common classifiers: 1) Bayesian linear discriminant analysis; 2) multilayer perceptron (MLP); and 3) support vector machines. Prior to classification, the data were spatially filtered with xDAWN (for the maximization of the signal-to-signal-plus-noise ratio), common spatial pattern, or not spatially filtered. The 12 analytical techniques were tested on EEG data recorded in three rapid serial visual presentation experiments that required the observer to discriminate rare target stimuli from frequent nontarget stimuli. Classification performance discriminating targets from nontargets depended on both the spatial filtering method and the classifier. In addition, the nonlinear classifier MLP outperformed the linear methods. Finally, training based AUC maximization provided better performance than training based on the minimization of the mean square error. The results support the conclusion that the choice of the systems architecture is critical and both spatial filtering and classification must be considered together.
C1 [Cecotti, Hubert; Eckstein, Miguel P.; Giesbrecht, Barry] Univ Calif Santa Barbara, Dept Psychol & Brain Sci, Inst Collaborat Biotechnol, Santa Barbara, CA 93106 USA.
   [Cecotti, Hubert] Univ Ulster, Sch Comp & Intelligent Syst, Coleraine BT48 7JL, Londonderry, North Ireland.
   [Cecotti, Hubert] Univ Henri Poincare, Nancy, France.
   [Cecotti, Hubert] ESIAL, Nancy, France.
   [Cecotti, Hubert] Univ Bremen, Inst Automat, D-28359 Bremen, Germany.
   [Cecotti, Hubert] CNRS, Gipsa Lab, Grenoble, France.
   [Cecotti, Hubert; Eckstein, Miguel P.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA.
   [Eckstein, Miguel P.] Cedars Sinai Med Ctr, Dept Med Phys & Imaging, Los Angeles, CA USA.
   [Eckstein, Miguel P.] NASA, Ames Res Ctr, Mountain View, CA USA.
   [Giesbrecht, Barry] Univ Calif Santa Barbara, Dept Psychol & Brain Sci, Santa Barbara, CA 93106 USA.
RP Cecotti, H (reprint author), Univ Calif Santa Barbara, Dept Psychol & Brain Sci, Inst Collaborat Biotechnol, Santa Barbara, CA 93106 USA.
EM hub20xx@hotmail.com; eckstein@psych.ucsb.edu; giesbrecht@psych.ucsb.edu
FU Institute for Collaborative Biotechnologies through the U.S. Army
   Research Office [W911NF-09-D-0001]
FX This work was supported by the Institute for Collaborative
   Biotechnologies under Contract W911NF-09-D-0001 through the U.S. Army
   Research Office.
NR 61
TC 6
Z9 6
U1 6
U2 29
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2162-237X
EI 2162-2388
J9 IEEE T NEUR NET LEAR
JI IEEE Trans. Neural Netw. Learn. Syst.
PD NOV
PY 2014
VL 25
IS 11
BP 2030
EP 2042
DI 10.1109/TNNLS.2014.2302898
PG 13
WC Computer Science, Artificial Intelligence; Computer Science, Hardware &
   Architecture; Computer Science, Theory & Methods; Engineering,
   Electrical & Electronic
SC Computer Science; Engineering
GA AS2DJ
UT WOS:000344089300007
PM 25330426
ER

PT J
AU Soltani, A
   Akbarzadeh-T, MR
AF Soltani, Azadeh
   Akbarzadeh-T, M. -R.
TI Confabulation-Inspired Association Rule Mining for Rare and Frequent
   Itemsets
SO IEEE TRANSACTIONS ON NEURAL NETWORKS AND LEARNING SYSTEMS
LA English
DT Article
DE Association rule mining (ARM); associative classification; cogency;
   confabulation theory; rare item mining
ID SELF-ORGANIZING MAPS; DENSITY-ESTIMATION; ALGORITHMS; MECHANISM;
   NETWORKS; SUPPORT
AB A new confabulation-inspired association rule mining (CARM) algorithm is proposed using an interestingness measure inspired by cogency. Cogency is only computed based on pairwise item conditional probability, so the proposed algorithm mines association rules by only one pass through the file. The proposed algorithm is also more efficient for dealing with infrequent items due to its cogency-inspired approach. The problem of associative classification is used here for evaluating the proposed algorithm. We evaluate CARM over both synthetic and real benchmark data sets obtained from the UC Irvine machine learning repository. Experiments show that the proposed algorithm is consistently faster due to its one time file access and consumes less memory space than the Conditional Frequent Patterns growth algorithm. In addition, statistical analysis reveals the superiority of the approach for classifying minority classes in unbalanced data sets.
C1 [Soltani, Azadeh; Akbarzadeh-T, M. -R.] Ferdowsi Univ Mashhad, Ctr Excellence Soft Comp & Intelligent Informat P, Dept Comp Engn, Mashhad 917751111, Iran.
   [Akbarzadeh-T, M. -R.] Ferdowsi Univ Mashhad, Ctr Excellence Soft Comp & Intelligent Informat P, Dept Elect Engn, Mashhad 917751111, Iran.
   [Soltani, Azadeh] Azad Univ Bojnourd, Bojnourd, Iran.
   [Soltani, Azadeh] Bojnourd Univ, Bojnourd, Iran.
   [Akbarzadeh-T, M. -R.] UNM, NASA, Ctr Autonomous Control Engn, Albuquerque, NM USA.
RP Soltani, A (reprint author), Ferdowsi Univ Mashhad, Ctr Excellence Soft Comp & Intelligent Informat P, Dept Comp Engn, Mashhad 917751111, Iran.
EM soltani.az@stu-mail.um.ac.ir; akbarzadeh@ieee.org
NR 45
TC 2
Z9 2
U1 1
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2162-237X
EI 2162-2388
J9 IEEE T NEUR NET LEAR
JI IEEE Trans. Neural Netw. Learn. Syst.
PD NOV
PY 2014
VL 25
IS 11
BP 2053
EP 2064
DI 10.1109/TNNLS.2014.2303137
PG 12
WC Computer Science, Artificial Intelligence; Computer Science, Hardware &
   Architecture; Computer Science, Theory & Methods; Engineering,
   Electrical & Electronic
SC Computer Science; Engineering
GA AS2DJ
UT WOS:000344089300009
PM 25330428
ER

PT J
AU Berg, A
   Lintner, BR
   Findell, KL
   Malyshev, S
   Loikith, PC
   Gentine, P
AF Berg, Alexis
   Lintner, Benjamin R.
   Findell, Kirsten L.
   Malyshev, Sergey
   Loikith, Paul C.
   Gentine, Pierre
TI Impact of Soil Moisture-Atmosphere Interactions on Surface Temperature
   Distribution
SO JOURNAL OF CLIMATE
LA English
DT Article
ID PART I; CLIMATE PREDICTABILITY; DATA ASSIMILATION; EARTH-SYSTEM; LAND;
   PRECIPITATION; EXTREMES; FEEDBACK; SCALE; VARIABILITY
AB Understanding how different physical processes can shape the probability distribution function (PDF) of surface temperature, in particular the tails of the distribution, is essential for the attribution and projection of future extreme temperature events. In this study, the contribution of soil moisture-atmosphere interactions to surface temperature PDFs is investigated. Soil moisture represents a key variable in the coupling of the land and atmosphere, since it controls the partitioning of available energy between sensible and latent heat flux at the surface. Consequently, soil moisture variability driven by the atmosphere may feed back onto the near-surface climate-in particular, temperature. In this study, two simulations of the current-generation Geophysical Fluid Dynamics Laboratory (GFDL) Earth System Model, with and without interactive soil moisture, are analyzed in order to assess how soil moisture dynamics impact the simulated climate. Comparison of these simulations shows that soil moisture dynamics enhance both temperature mean and variance over regional "hotspots" of land atmosphere coupling. Moreover, higher-order distribution moments, such as skewness and kurtosis, are also significantly impacted, suggesting an asymmetric impact on the positive and negative extremes of the temperature PDF. Such changes are interpreted in the context of altered distributions of the surface turbulent and radiative fluxes. That the moments of the temperature distribution may respond differentially to soil moisture dynamics underscores the importance of analyzing moments beyond the mean and variance to characterize fully the interplay of soil moisture and near-surface temperature. In addition, it is shown that soil moisture dynamics impacts daily temperature variability at different time scales over different regions in the model.
C1 [Berg, Alexis; Lintner, Benjamin R.] Rutgers State Univ, New Brunswick, NJ 08903 USA.
   [Berg, Alexis; Findell, Kirsten L.] Geophys Fluid Dynam Lab, Princeton, NJ USA.
   [Malyshev, Sergey] Princeton Univ, Princeton, NJ 08544 USA.
   [Loikith, Paul C.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Gentine, Pierre] Columbia Univ, New York, NY USA.
RP Berg, A (reprint author), Columbia Univ, Earth Inst, Int Res Climate & Soc IRI, 61 Rt 9W, Palisades, NY 10964 USA.
EM aberg@iri.columbia.edu
FU National Science Foundation (NSF) [AGS-1035968, AGS-1035843]; New Jersey
   Agricultural Experiment Station Hatch Grant [NJ07102]; NSF Postdoctoral
   Fellowship [AGS-1331375]; National Oceanic and Atmospheric (U.S.
   Department of Commerce) [NA08OAR4320752]; U.S. Department of Agriculture
   [2011-67003-30373]; Carbon Mitigation Initiative at Princeton University
   - British Petroleum
FX This work was supported by National Science Foundation (NSF) Grants
   AGS-1035968 and AGS-1035843 and New Jersey Agricultural Experiment
   Station Hatch Grant NJ07102. A.B. is currently supported by NSF
   Postdoctoral Fellowship AGS-1331375. S.M. acknowledges support from the
   National Oceanic and Atmospheric (U.S. Department of Commerce) Grant
   NA08OAR4320752, U.S. Department of Agriculture Grant 2011-67003-30373,
   and the Carbon Mitigation Initiative at Princeton University, sponsored
   by British Petroleum. Part of this research was carried out at the Jet
   Propulsion Laboratory, California Institute of Technology, under a
   contract with the National Aeronautics and Space Administration. The
   authors thank Sonia Seneviratne for her comments on the manuscript.
NR 51
TC 15
Z9 15
U1 2
U2 32
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 NOV 1
PY 2014
VL 27
IS 21
BP 7976
EP 7993
DI 10.1175/JCLI-D-13-00591.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS2TE
UT WOS:000344131500002
ER

PT J
AU Losee, JP
   Fisher, J
   Teel, DJ
   Baldwin, RE
   Marcogliese, DJ
   Jacobson, KC
AF Losee, J. P.
   Fisher, J.
   Teel, D. J.
   Baldwin, R. E.
   Marcogliese, D. J.
   Jacobson, K. C.
TI Growth and condition of juvenile coho salmon Oncorhynchus kisutch relate
   positively to species richness of trophically transmitted parasites
SO JOURNAL OF FISH BIOLOGY
LA English
DT Article
DE fresh water; habitat quality; IGF1; marine; species diversity
ID NORTHERN CALIFORNIA CURRENT; CHINOOK SALMON; PACIFIC SALMON; COMPONENT
   COMMUNITIES; MARINE ECOSYSTEMS; O-TSHAWYTSCHA; BALTIC SEA; FOOD WEBS;
   FISH; OREGON
AB The aims of this study were first, to test the hypothesis that metrics of fish growth and condition relate positively to parasite species richness (S-R) in a salmonid host; second, to identify whether S-R differs as a function of host origin; third, to identify whether acquisition of parasites through marine v. freshwater trophic interactions was related to growth and condition of juvenile salmonids. To evaluate these questions, species diversity of trophically transmitted parasites in juvenile coho salmon Oncorhynchus kisutch collected off the coast of the Oregon and Washington states, U.S.A. in June 2002 and 2004 were analysed. Fish infected with three or more parasite species scored highest in metrics of growth and condition. Fish originating from the Columbia River basin had lower S-R than those from the Oregon coast, Washington coast and Puget Sound, WA. Parasites obtained through freshwater or marine trophic interactions were equally important in the relationship between S-R and ocean growth and condition of juvenile O. kisutch salmon. (C) 2014 The Fisheries Society of the British Isles
C1 [Losee, J. P.] Washington Dept Fish & Wildlife, Fish Program, Olympia, WA 98502 USA.
   [Fisher, J.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
   [Teel, D. J.] NOAA, Manchester Res Stn, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Manchester, WA 98353 USA.
   [Baldwin, R. E.] Alberta Govt, Fish & Wildlife, Ft Mcmurray, AB T9H 2K4, Canada.
   [Marcogliese, D. J.] Environm Canada, Watershed Hydrol & Ecol Res Div, Water Sci & Technol Directorate,St Lawrence Ctr, Aquat Biodivers Sect,Sci & Technol Branch, Montreal, PQ H2Y 2E7, Canada.
   [Jacobson, K. C.] NOAA, Newport Res Stn, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
RP Losee, JP (reprint author), Washington Dept Fish & Wildlife, Fish Program, Olympia, WA 98502 USA.
EM james.losee@dfw.wa.gov
FU Bonneville Power Administration; NOAA Fisheries
FX We would like to thank K. Cooper from the NWFSC for running IGF1 assays,
   A. Claxton for his expertise in parasite identification, A. Claiborne
   for statistical assistance and T. Hurst, L. Weitkamp, M. B. Rew and K.
   Losee for revision of an early draft of this manuscript. We particularly
   thank the crew and scientists of the F. V. Frosti who assisted in
   collection of samples. Funding was provided by the Bonneville Power
   Administration and NOAA Fisheries.
NR 58
TC 1
Z9 1
U1 3
U2 18
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-1112
EI 1095-8649
J9 J FISH BIOL
JI J. Fish Biol.
PD NOV
PY 2014
VL 85
IS 5
BP 1665
EP 1681
DI 10.1111/jfb.12525
PG 17
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA AS0MF
UT WOS:000343970400022
PM 25271907
ER

PT J
AU Morgan, D
   Chung, SJ
   Hadaegh, FY
AF Morgan, Daniel
   Chung, Soon-Jo
   Hadaegh, Fred Y.
TI Model Predictive Control of Swarms of Spacecraft Using Sequential Convex
   Programming
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article; Proceedings Paper
CT AIAA/AAS Astrodynamics Specialist Conference
CY AUG 13-16, 2012
CL Minneapolis, MN
SP AIAA, AAS
ID FORMATION-FLYING SPACECRAFT; RECEDING HORIZON CONTROL; SATELLITE
   CLUSTERS; ALGORITHM; SYSTEMS; GUIDANCE; MOTION; SDPT3
AB This paper presents a decentralized, model predictive control algorithm for the optimal guidance and reconfiguration of swarms of spacecraft composed of hundreds to thousands of agents with limited capabilities. In previous work, J(2)-invariant orbits have been found to provide collision-free motion for hundreds of orbits in a low Earth orbit. This paper develops real-time optimal control algorithms for the swarm reconfiguration that involve transferring from one J(2)-invariant orbit to another while avoiding collisions and minimizing fuel. The proposed model predictive control-sequential convex programming algorithm uses sequential convex programming to solve a series of approximate path planning problems until the solution converges. By updating the optimal trajectories during the reconfiguration, the model predictive control algorithm results in decentralized computations and communication between neighboring spacecraft only. Additionally, model predictive control reduces the horizon of the convex optimizations, which reduces the run time of the algorithm. Multiple time steps, time-varying collision constraints, and communication requirements are developed to guarantee stability, feasibility, and robustness of the model predictive control-sequential convex programming algorithm.
C1 [Morgan, Daniel; Chung, Soon-Jo] Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.
   [Hadaegh, Fred Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Morgan, D (reprint author), Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.
EM morgan29@illinois.edu; sjchung@illinois.edu; fred.y.hadaegh@jpl.nasa.gov
OI Chung, Soon-Jo/0000-0002-6657-3907
NR 46
TC 17
Z9 19
U1 4
U2 17
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 NOV
PY 2014
VL 37
IS 6
BP 1725
EP 1740
DI 10.2514/1.G000218
PG 16
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA AR9UP
UT WOS:000343924400001
ER

PT J
AU Aldrich, JB
AF Aldrich, Jack B.
TI Attitude Control with Analytic Disturbance-Rejection Guarantee
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID CONTROL LAWS; GLOBAL STABILIZATION; QUATERNION FEEDBACK; RIGID
   SPACECRAFT; ERROR DYNAMICS; TRACKING; MANEUVERS
AB Analytic formulas that guarantee a minimum level of disturbance-rejection performance are derived for a class of attitude control problems consisting of linear proportional-derivative quaternion feedback applied to a rigid-body spacecraft plant model. Specifically, a Lyapunov-based disturbance-rejection assessment tool is derived for a general class of perturbed nonlinear systems, and then it is specialized to the linear attitude control class. Although the tool accepts generic Lyapunov function candidates, this paper demonstrates that existing Lyapunov functions (that readily prove asymptotic stability for attitude control systems) are insufficiently parameterized for purposes of estimating disturbance-rejection capability via the proposed tool. In response to this shortcoming, two new Lyapunov functions are proposed, and they are evaluated in the context of two closed-form disturbance-rejection performance assessment algorithms. Both algorithms demonstrate that the magnitude of the allowable disturbance torque is proportional to 1) the magnitude of the allowable angular accuracy, 2) the square of the control bandwidth, and 3) the minimum eigenvalue of the spacecraft inertia matrix. Moreover, the constant of proportionality (coefficient of rejection) is shown to degrade gradually for larger angles, and it eventually goes to zero as the user-specified angular accuracy is increased to 180 deg (for a high-order Lyapunov function) and 12 deg (for a low-order quadratic Lyapunov function).
C1 CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, Pasadena, CA 91109 USA.
RP Aldrich, JB (reprint author), CALTECH, Jet Prop Lab, Guidance & Control Anal Grp, 4800 Oak Grove Dr,M-S 198-326, Pasadena, CA 91109 USA.
FU Jet Propulsion Laboratory, California Institute of Technology
FX Government sponsorship is acknowledged. The research described in this
   paper was carried out at the Jet Propulsion Laboratory, California
   Institute of Technology, under a contract with NASA. The author
   acknowledges 1) helpful discussions with David S. Bayard and Milan
   Mandic, and 2) constructive comments from the anonymous reviewers.
NR 34
TC 0
Z9 0
U1 1
U2 12
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 NOV
PY 2014
VL 37
IS 6
BP 1791
EP 1807
DI 10.2514/1.G000339
PG 17
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA AR9UP
UT WOS:000343924400006
ER

PT J
AU Bandyopadhyay, A
   Majumdar, A
AF Bandyopadhyay, Alak
   Majumdar, Alok
TI Network Flow Simulation of Fluid Transients in Rocket Propulsion Systems
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
ID PROPELLANT FEED SYSTEM; FRICTION; PIPE
AB This paper presents a numerical study of fluid transients in a pipeline with the sudden opening of a valve. A network flow simulation software (Generalized Fluid System Simulation Program) based on the finite volume method has been used to predict the pressure surges in a pipeline that has entrapped air at one end of the pipe. The mathematical model is formulated by involving the flow equations in the liquid (water) zone and compressibility of the entrapped air. The numerical results are compared with the experimental data available in the literature. The study is conducted for a range of the reservoir pressure and for different amounts of initial air present in the pipeline. The numerical results compare well within reasonable accuracy (less than 8%) for a range of inlet-to-initial pressure ratios when the amount of air present is relatively high (alpha approximate to 0.45). A fast Fourier transform is performed on the pressure oscillations to predict the various modal frequencies of the pressure wave.
C1 [Bandyopadhyay, Alak] Alabama A&M Univ, Dept Elect Engn & Comp Sci, Normal, AL 35762 USA.
   [Majumdar, Alok] NASA, George C Marshall Space Flight Ctr, Thermal & Combust Anal Branch, Huntsville, AL 35812 USA.
RP Bandyopadhyay, A (reprint author), Alabama A&M Univ, Dept Elect Engn & Comp Sci, 4900 Meridian St, Normal, AL 35762 USA.
EM alak.bando@aamu.edu; alok.k.majumdar@nasa.gov
FU NASA Summer Faculty program
FX This work was supported by a fellowship awarded to Alak Bandyoadhyay
   under the NASA Summer Faculty program. The work was conducted at NASA
   Marshall Space Flight Center in Huntsville, Alabama, in the ER43/Thermal
   Analysis Branch. The authors would like to thank the Publications Office
   of the NASA Marshall Space Flight Center for the preparation of this
   manuscript.
NR 19
TC 1
Z9 1
U1 0
U2 2
PU AMER INST AERONAUTICS  ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
EI 1533-3876
J9 J PROPUL POWER
JI J. Propul. Power
PD NOV-DEC
PY 2014
VL 30
IS 6
BP 1646
EP 1653
DI 10.2514/1.B35194
PG 8
WC Engineering, Aerospace
SC Engineering
GA AS2ZM
UT WOS:000344145000025
ER

PT J
AU Wang, TS
   Zhao, X
   Zhang, SJ
   Chen, YS
AF Wang, Ten-See
   Zhao, Xiang
   Zhang, Sijun
   Chen, Yen-Sen
TI Development of an Aeroelastic Modeling Capability for Transient Nozzle
   Flow Analysis
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
ID SIDE-LOAD ANALYSIS; FILM-COOLED NOZZLES; ENGINE NOZZLE; SEPARATION;
   PERFORMANCE; SIMULATION; REGIME
AB Lateral nozzle forces are known to cause severe structural damage to any new rocket engine in development during testing. Although three-dimensional, transient, turbulent, chemically reacting computational fluid dynamics methodology has been demonstrated to capture major side load physics with rigid nozzles, hot-fire tests often show nozzle structure deformation during major side load events, leading to structural damages if structural strengthening measures were not taken. The modeling picture is incomplete without the capability to address the two-way responses between the structure and fluid. The objective of this study is to develop a coupled aeroelastic modeling capability by implementing the necessary structural dynamics component into an anchored computational fluid dynamics methodology. The computational fluid dynamics component is based on an unstructured-grid pressure-based computational fluid dynamics formulation, whereas the computational structural dynamics component is developed under the framework of modal analysis. Transient aeroelastic nozzle startup analyses at sea level were performed to demonstrate the successful simulation of nozzle wall deformation with the proposed tightly coupled algorithm, and the computed results pertinent to fluid-structure interaction presented.
C1 [Wang, Ten-See] NASA, George C Marshall Space Flight Ctr, Fluid Dynam Branch, Prop Struct Thermal & Fluids Anal Div, Huntsville, AL 35812 USA.
   [Zhao, Xiang] Alabama A&M Univ, Huntsville, AL 35762 USA.
   [Zhang, Sijun] ESI CFD Inc, Huntsville, AL 35806 USA.
   [Chen, Yen-Sen] Appl Res Lab, Hsinchu 30078, Taiwan.
RP Wang, TS (reprint author), NASA, George C Marshall Space Flight Ctr, Fluid Dynam Branch, Prop Struct Thermal & Fluids Anal Div, ER42, Huntsville, AL 35812 USA.
FU J-2X engine program at NASA Marshall Space Flight Center; National
   Science Foundation; NASA Summer Faculty Fellowship
FX The first author was partially supported by the J-2X engine program at
   NASA Marshall Space Flight Center, where Mike Shadoan managed the nozzle
   project and Marcus Neely managed the system test project. X. Zhao was
   partially supported by a Seed Grant from the National Science Foundation
   and by a NASA 2012 Summer Faculty Fellowship. The authors acknowledge
   James Beck of Pratt and Whitney Rocketdyne for his insight in
   fluid-structure interactions. The authors also wish to thank Eric Blades
   of ATA Engineering for several initial discussions.
NR 37
TC 0
Z9 0
U1 0
U2 5
PU AMER INST AERONAUTICS  ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
EI 1533-3876
J9 J PROPUL POWER
JI J. Propul. Power
PD NOV-DEC
PY 2014
VL 30
IS 6
BP 1692
EP 1700
DI 10.2514/1.B35277
PG 9
WC Engineering, Aerospace
SC Engineering
GA AS2ZM
UT WOS:000344145000030
ER

PT J
AU Prive, NC
   Xie, YF
   Koch, S
   Atlas, R
   Majumdar, SJ
   Hoffman, RN
AF Prive, N. C.
   Xie, Yuanfu
   Koch, Steven
   Atlas, Robert
   Majumdar, Sharanya J.
   Hoffman, Ross N.
TI An Observing System Simulation Experiment for the Unmanned Aircraft
   System Data Impact on Tropical Cyclone Track Forecasts
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID SYNOPTIC SURVEILLANCE
AB High-altitude, long-endurance unmanned aircraft systems (HALE UAS) are capable of extended flights for atmospheric sampling. A case study was conducted to evaluate the potential impact of dropwindsonde observations from HALE UAS on tropical cyclone track prediction; tropical cyclone intensity was not addressed. This study employs a global observing system simulation experiment (OSSE) developed at the National Oceanic and Atmospheric Administration/Earth System Research Laboratory (NOAA/ESRL) that is based on the NOAA/National Centers for Environmental Prediction gridpoint statistical interpolation (GSI) data assimilation system and Global Forecast System (GFS) model. Different strategies for dropwindsonde deployment and UAS flight paths were compared. The introduction of UAS-deployed dropwindsondes was found to consistently improve the track forecast skill during the early forecast up to 96 h, with the caveat that the experiments omitted both vortex relocation and dropwindsondes from manned flights in the tropical cyclone region. The more effective UAS dropvvindsonde deployment patterns sampled both the environment and the body of the tropical cyclone.
C1 [Prive, N. C.] Colorado State Univ, Cooperat Inst Res Atmosphere, Boulder, CO USA.
   [Xie, Yuanfu] NOAA, Global Syst Div, Earth Syst Res Lab, Boulder, CO USA.
   [Koch, Steven] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA.
   [Atlas, Robert] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA.
   [Majumdar, Sharanya J.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Meteorol & Phys Oceanog, Miami, FL 33149 USA.
   [Hoffman, Ross N.] Univ Miami, Cooperat Inst Marine & Atmospher Studies, Miami, FL USA.
RP Prive, NC (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM nikki.prive@nasa.gov
RI Atlas, Robert/A-5963-2011; Xie, Yuanfu/G-4413-2015
OI Atlas, Robert/0000-0002-0706-3560; 
FU NOAA/UAS Program
FX This work was supported by Dr. Robbie Hood and the NOAA/UAS Program.
   Additional support was provided by Dr. John Cortinas of the NOAA/Office
   of Weather and Air Quality. The ECMWF Nature Run was provided by Erik
   Andersson through arrangements made by Michiko Masutani.
NR 12
TC 3
Z9 3
U1 0
U2 7
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 NOV
PY 2014
VL 142
IS 11
BP 4357
EP 4363
DI 10.1175/MWR-D-14-00197.1
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS4BW
UT WOS:000344219400023
ER

PT J
AU Williams, D
   Arvidson, T
   Irons, J
   Rocchio, L
   Russell, C
   Goward, S
AF Williams, Darrel
   Arvidson, Terry
   Irons, Jim
   Rocchio, Laura
   Russell, Carol
   Goward, Sam
CA Landsat Legacy Project Team
TI LANDSAT LEGACY PROJECT
SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING
LA English
DT Editorial Material
C1 [Williams, Darrel] Global Sci & Technol, Washington, DC USA.
   [Arvidson, Terry] Lockheed Martin, Bethesda, MD USA.
   [Irons, Jim] NASA GSFC, Greenbelt, MD USA.
   [Russell, Carol] Sci Syst & Applicat Inc, Hampton, VA USA.
   [Goward, Sam] Univ Maryland, College Pk, MD USA.
NR 0
TC 0
Z9 0
U1 2
U2 4
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 NOV
PY 2014
VL 80
IS 11
BP 1014
EP 1016
PG 3
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
   Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
   Photographic Technology
GA AS4BR
UT WOS:000344219000003
ER

PT J
AU Stavros, EN
   McKenzie, D
   Larkin, N
AF Stavros, E. Natasha
   McKenzie, Donald
   Larkin, Narasimhan
TI The climate-wildfire-air quality system: interactions and feedbacks
   across spatial and temporal scales
SO WILEY INTERDISCIPLINARY REVIEWS-CLIMATE CHANGE
LA English
DT Review
ID SOUTHERN CALIFORNIA WILDFIRES; WESTERN UNITED-STATES; FOREST-FIRES;
   MEDITERRANEAN ECOSYSTEMS; WASHINGTON-STATE; CHANGING CLIMATE; PONDEROSA
   PINE; PROCESS MODELS; WILDLAND FIRE; VEGETATION
AB Future climate change and its effects on social and ecological systems present challenges for preserving valued ecosystem services, including local and regional air quality. Wildfire is a major source of air-quality impact in some locations, and a substantial contributor to pollutants of concern, including nitrogen oxides and particulate matter, which are regulated to protect public and environmental health. Since climate change is expected to increase total area burned by wildfire and wildfires affect air quality, which is regulated, there is a need to define and study climate, wildfire, and air quality as one system. We review interactions and feedbacks acting across space and time within the climate-wildfire-air quality system, providing a foundation for integrated modeling and for assessing the ecological and social impacts of this system and its broader ecological, social, and scientific implications. (C) 2014 John Wiley & Sons, Ltd.
C1 [Stavros, E. Natasha] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
   [McKenzie, Donald; Larkin, Narasimhan] Univ Washington, USDA Forest Serv, Pacific Wildland Fire Sci Lab, Seattle, WA 98195 USA.
RP Stavros, EN (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Natasha.Stavros@jpl.nasa.gov
FU Pacific Northwest Research Station, U.S. Forest Service; EPA-STAR
   program; Joint Fire Science Program [11-1-7-4, 12-S-01-2]; National
   Aeronautics and Space Administration
FX Funding for this review has been provided by the Pacific Northwest
   Research Station, U.S. Forest Service; the EPA-STAR program; and the
   Joint Fire Science Program, project # 11-1-7-4 and # 12-S-01-2. Many
   thanks for constructive reviews from Ernesto Alvarado, Christian
   Torgersen, Tim Essington, David L. Peterson, and Tara Strand. The final
   stages of this research were carried out at the Jet Propulsion
   Laboratory, California Institute of Technology, under a contract with
   the National Aeronautics and Space Administration.
NR 107
TC 3
Z9 3
U1 2
U2 30
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1757-7780
EI 1757-7799
J9 WIRES CLIM CHANGE
JI Wiley Interdiscip. Rev.-Clim. Chang.
PD NOV-DEC
PY 2014
VL 5
IS 6
BP 719
EP 733
DI 10.1002/wcc.303
PG 15
WC Environmental Studies; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AS6CZ
UT WOS:000344353600003
ER

PT J
AU Richard, EE
   Davis, JR
AF Richard, Elizabeth E.
   Davis, Jeffrey R.
TI NASA Human Health and Performance Center: Open innovation successes and
   collaborative projects
SO ACTA ASTRONAUTICA
LA English
DT Article
DE NHHPC; Collaboration; Innovation; Health; Engagement
AB In May 2007, what was then the Space Life Sciences Directorate published the 2007 Space Life Sciences Strategy for Human Space Exploration, setting the course for development and implementation of new business models and significant advances in external collaboration over the next five years. The strategy was updated on the basis of these accomplishments and reissued as the NASA Human Health and Performance Strategy in 2012, and continues to drive new approaches to innovation for the directorate. This short paper describes the successful execution of the strategy, driving organizational change through open innovation efforts and collaborative projects, including efforts of the NASA Human Health and Performance Center (NHHPC). (C) 2014 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Richard, Elizabeth E.] Wyle, Houston, TX 77058 USA.
   [Davis, Jeffrey R.] NASA, Houston, TX 77058 USA.
RP Richard, EE (reprint author), Wyle, 1290 Hercules Ave, Houston, TX 77058 USA.
EM erichard@wylehou.com; jeffrey.r.davis@nasa.gov
NR 1
TC 0
Z9 0
U1 2
U2 28
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 NOV
PY 2014
VL 104
IS 1
SI SI
BP 383
EP 387
DI 10.1016/j.actaastro.2014.05.010
PG 5
WC Engineering, Aerospace
SC Engineering
GA AR8RH
UT WOS:000343841700039
ER

PT J
AU Schatzman, D
   Wilson, J
   Arad, E
   Seifert, A
   Shtendel, T
AF Schatzman, David
   Wilson, Jacob
   Arad, Eran
   Seifert, Avraham
   Shtendel, Tom
TI Drag-Reduction Mechanisms of Suction-and-Oscillatory-Blowing Flow
   Control
SO AIAA JOURNAL
LA English
DT Article
ID HIGH REYNOLDS-NUMBERS; SEPARATION CONTROL; PART 1
AB An active-flow-control study, using steady suction-and-oscillatory-blowing actuators, was conducted on an axisymmetric bluff-body model for a range of Reynolds numbers between 2 x 10(6) and 5 x 10(6). Previous work on the same model demonstrated the experimental implementation and efficient drag reduction of the suction-and-oscillatory-blowing actuator system, including comparisons to computational fluid dynamics results. The current study presents a detailed analysis of the experimental data, coupled with a refined computational model toward a flow-physics understanding of the drag-reduction mechanisms of the suction-and-oscillatory-blowing active-flow-control system. The boundary-layer response was examined using time-averaged and phase-averaged hot-wire measurements conducted on the aft portion of the model where active flow control was applied. The drag-reduction behavior was scaled using multiple active-flow-control parameters associated with the unique and complex features of the suction-and-oscillatory-blowing active-flow-control system. The results show that the drag-reduction mechanisms associated with the suction-and-oscillatory-blowing actuation system include boundary-layer suction, wall-jet momentum addition, unsteady shear-layer excitation, the generation of thrust, and streamwise vortices.
C1 [Schatzman, David] Sci & Technol Corp, Moffett Field, CA 94035 USA.
   [Wilson, Jacob] US Army Res Dev & Engn Command, Moffett Field, CA 94035 USA.
   [Arad, Eran] RAFAEL Adv Def Syst Ltd, CFD, IL-31021 Haifa, Israel.
   [Seifert, Avraham; Shtendel, Tom] Tel Aviv Univ, Fac Engn, Sch Mech Engn, IL-69978 Tel Aviv, Israel.
RP Schatzman, D (reprint author), NASA, Ames Res Ctr, US Army Aviat Dev Directorate, Aeroflightdynam Directorate, Washington, DC 20024 USA.
NR 23
TC 2
Z9 2
U1 2
U2 16
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 NOV
PY 2014
VL 52
IS 11
BP 2491
EP 2505
DI 10.2514/1.J052903
PG 15
WC Engineering, Aerospace
SC Engineering
GA AR8AX
UT WOS:000343799000011
ER

PT J
AU Chemyakin, E
   Muller, D
   Burton, S
   Kolgotin, A
   Hostetler, C
   Ferrare, R
AF Chemyakin, Eduard
   Mueller, Detlef
   Burton, Sharon
   Kolgotin, Alexei
   Hostetler, Chris
   Ferrare, Richard
TI Arrange and average algorithm for the retrieval of aerosol parameters
   from multiwavelength high-spectral-resolution lidar/Raman lidar data
SO APPLIED OPTICS
LA English
DT Article
ID MICROPHYSICAL PARTICLE PARAMETERS; PRINCIPAL COMPONENT ANALYSIS;
   TROPOSPHERIC AEROSOL; OPTICAL-PROPERTIES; INVERSION; REGULARIZATION;
   BACKSCATTER; EXTINCTION
AB We present the results of a feasibility study in which a simple, automated, and unsupervised algorithm, which we call the arrange and average algorithm, is used to infer microphysical parameters (complex refractive index, effective radius, total number, surface area, and volume concentrations) of atmospheric aerosol particles. The algorithm uses backscatter coefficients at 355, 532, and 1064 nm and extinction coefficients at 355 and 532 nm as input information. Testing of the algorithm is based on synthetic optical data that are computed from prescribed monomodal particle size distributions and complex refractive indices that describe spherical, primarily fine mode pollution particles. We tested the performance of the algorithm for the "3 backscatter (beta)+2 (alpha) extinction (a)" configuration of a multiwavelength aerosol high-spectral-resolution lidar (HSRL) or Raman lidar. We investigated the degree to which the microphysical results retrieved by this algorithm depends on the number of input backscatter and extinction coefficients. For example, we tested " 3 beta + 1 alpha," "2 beta + 1 alpha" and "3 beta" 1a," lidar configurations. This arrange and average algorithm can be used in two ways. First, it can be applied for quick data processing of experimental data acquired with lidar. Fast automated retrievals of microphysical particle properties are needed in view of the enormous amount of data that can be acquired by the NASA Langley Research Center's airborne "3 beta + 2 alpha" High-Spectral-Resolution Lidar (HSRL-2). It would prove useful for the growing number of ground-based multiwavelength lidar networks, and it would provide an option for analyzing the vast amount of optical data acquired with a future spaceborne multiwavelength lidar. The second potential application is to improve the microphysical particle characterization with our existing inversion algorithm that uses Tikhonov's inversion with regularization. This advanced algorithm has recently undergone development to allow automated and unsupervised processing; the arrange and average algorithm can be used as a preclassifier to further improve its speed and precision. First tests of the performance of arrange and average algorithm are encouraging. We used a set of 48 different monomodal particle size distributions, 4 real parts and 15 imaginary parts of the complex refractive index. All in all we tested 2880 different optical data sets for 0%, 10%, and 20% Gaussian measurement noise (one-standard deviation). In the case of the "3 beta + 2 alpha" configuration with 10% measurement noise, we retrieve the particle effective radius to within 27% for 1964 (68.2%) of the test optical data sets. The number concentration is obtained to 76%, the surface area concentration to 16%, and the volume concentration to 30% precision. The "3 beta" configuration performs significantly poorer. The performance of the "3 beta + 1 alpha" and "2 beta +1 alpha"configurations is intermediate between the "3 beta + 2 alpha" and the "3 beta". (C) 2014 Optical Society of America
C1 [Chemyakin, Eduard; Mueller, Detlef] Sci Syst & Applicat Inc, NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Mueller, Detlef] Univ Hertfordshire, Hatfield AL10 9AB, Herts, England.
   [Burton, Sharon; Hostetler, Chris; Ferrare, Richard] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Kolgotin, Alexei] Phys Instrumentat Ctr, AM Prokhorov Gen Phys Inst, Troitsk 142190, Moscow Region, Russia.
RP Chemyakin, E (reprint author), Sci Syst & Applicat Inc, NASA, Langley Res Ctr, Mail Stop 475, Hampton, VA 23681 USA.
EM eduard.chemyakin@ssaihq.com
RI MUELLER, DETLEF/F-1010-2015
OI MUELLER, DETLEF/0000-0002-0203-7654
NR 19
TC 7
Z9 8
U1 2
U2 9
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 NOV 1
PY 2014
VL 53
IS 31
BP 7252
EP 7266
DI 10.1364/AO.53.007252
PG 15
WC Optics
SC Optics
GA AR9TL
UT WOS:000343919400023
PM 25402885
ER

PT J
AU Edelson, R
   Vaughan, S
   Malkan, M
   Kelly, BC
   Smith, KL
   Boyd, PT
   Mushotzky, R
AF Edelson, R.
   Vaughan, S.
   Malkan, M.
   Kelly, B. C.
   Smith, K. L.
   Boyd, P. T.
   Mushotzky, R.
TI DISCOVERY OF A similar to 5 DAY CHARACTERISTIC TIMESCALE IN THE KEPLER
   POWER SPECTRUM OF Zw 229-15
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; galaxies: active;
   galaxies: individual (Zw 229-15); galaxies: nuclei; galaxies: Seyfert
ID ACTIVE GALACTIC NUCLEI; X-RAY VARIABILITY; ACCRETION DISCS; BLACK-HOLES;
   XMM-NEWTON; RED NOISE; GALAXIES; REVERBERATION; PHOTOMETRY; SYSTEMS
AB We present time series analyses of the full Kepler data set of Zw 229-15. This Kepler light curve-with a baseline greater than 3 yr, composed of virtually continuous, evenly sampled 30 minute measurements-is unprecedented in its quality and precision. We utilize two methods of power spectral analysis to investigate the optical variability and search for evidence of a bend frequency associated with a characteristic optical variability timescale. Each method yields similar results. The first interpolates across data gaps to use the standard Fourier periodogram. The second, using the CARMA-based time-domain modeling technique of Kelly et al., does not need evenly sampled data. Both methods find excess power at high frequencies that may be due to Kepler instrumental effects. More importantly, both also show strong bends (Delta alpha similar to 2) at timescales of similar to 5 days, a feature similar to those seen in the X-ray power spectral densities of active galactic nuclei (AGNs) but never before in the optical. This observed similar to 5 day timescale may be associated with one of several physical processes potentially responsible for the variability. A plausible association could be made with light-crossing dynamical or thermal timescales depending on the assumed value of the accretion disk size and on unobserved disk parameters such as alpha and H/R. This timescale is not consistent with the viscous timescale, which would be years in a similar to 10(7)M(circle dot) AGN such as Zw 229-15. However, there must be a second bend on long (greater than or similar to 1 yr) timescales and that feature could be associated with the viscous timescale.
C1 [Edelson, R.; Smith, K. L.; Mushotzky, R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Vaughan, S.] Univ Leicester, Xray & Observat Astron Grp, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
   [Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
   [Kelly, B. C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
   [Boyd, P. T.] NASA, Astrophys Sci Div, GSFC, Greenbelt, MD 20771 USA.
RP Edelson, R (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM redelson@astro.umd.edu
FU NASA [NNX13AC26G, NNX13AE99G]
FX The authors appreciate the assistance of Martin Still and Tom Barclay of
   the Kepler GO office in helping us understand the Kepler data and Keith
   Horne and Qian Wang for sharing their unpublished results on Zw 229-15.
   We also thank the anonymous referee and the editors of The Astrophysical
   Journal for a prompt and helpful refereeing process. This research
   utilized the HEASARC, IRSA, NED, and MAST data archives and the NASA
   Astrophysics Data System Bibliographic Service. R. E. acknowledges
   support from the Kepler GO and ADAP programs through NASA grants
   NNX13AC26G and NNX13AE99G.
NR 34
TC 14
Z9 14
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 NOV 1
PY 2014
VL 795
IS 1
AR 2
DI 10.1088/0004-637X/795/1/2
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300002
ER

PT J
AU Erb, DK
   Steidel, CC
   Trainor, RF
   Bogosavljevic, M
   Shapley, AE
   Nestor, DB
   Kulas, KR
   Law, DR
   Strom, AL
   Rudie, GC
   Reddy, NA
   Pettini, M
   Konidaris, NP
   Mace, G
   Matthews, K
   McLean, IS
AF Erb, Dawn K.
   Steidel, Charles C.
   Trainor, Ryan F.
   Bogosavljevic, Milan
   Shapley, Alice E.
   Nestor, Daniel B.
   Kulas, Kristin R.
   Law, David R.
   Strom, Allison L.
   Rudie, Gwen C.
   Reddy, Naveen A.
   Pettini, Max
   Konidaris, Nicholas P.
   Mace, Gregory
   Matthews, Keith
   McLean, Ian S.
TI THE Ly alpha PROPERTIES OF FAINT GALAXIES AT z similar to 2-3 WITH
   SYSTEMIC REDSHIFTS AND VELOCITY DISPERSIONS FROM KECK-MOSFIRE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift
ID STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; MULTIPHASE
   INTERSTELLAR-MEDIUM; REST-FRAME ULTRAVIOLET; FORMATION RATE DENSITY;
   EMITTING GALAXIES; LUMINOSITY FUNCTION; STELLAR POPULATIONS; PHYSICAL
   ORIGIN; H-ALPHA
AB We study the Ly alpha profiles of 36 spectroscopically detected Ly alpha-emitters (LAEs) at z similar to 2-3, using Keck MOSFIRE to measure systemic redshifts and velocity dispersions from rest-frame optical nebular emission lines. The sample has a median optical magnitude R = 26.0, and ranges from R similar or equal to 23 to R > 27, corresponding to rest-frame UV absolute magnitudes M-UV similar or equal to -22 to M-UV > -18.2. Dynamical masses range from M-dyn < 1.3 x 10(8) M circle dot to M-dyn = 6.8 x 10(9) M circle dot, with a median value of M-dyn = 6.3 x 10(8) M circle dot. Thirty of the 36 Ly alpha emission lines are redshifted with respect to the systemic velocity with at least 1 sigma significance, and the velocity offset with respect to systemic Delta v(Ly alpha) is correlated with the R-band magnitude, M-UV, and the velocity dispersion measured from nebular emission lines with >3 sigma significance: brighter galaxies with larger velocity dispersions tend to have larger values of Delta v(Ly alpha). We also make use of a comparison sample of 122 UV-color-selected R < 25.5 galaxies at z similar to 2, all with Ly alpha emission and systemic redshifts measured from nebular emission lines. Using the combined LAE and comparison samples for a total of 158 individual galaxies, we find that Delta v(Ly alpha) is anti-correlated with the Ly alpha equivalent width with 7 sigma significance. Our results are consistent with a scenario in which the Ly alpha profile is determined primarily by the properties of the gas near the systemic redshift; in such a scenario, the opacity to Lya photons in lower mass galaxies may be reduced if large gaseous disks have not yet developed and if the gas is ionized by the harder spectrum of young, low metallicity stars.
C1 [Erb, Dawn K.] Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53211 USA.
   [Steidel, Charles C.; Trainor, Ryan F.; Strom, Allison L.; Konidaris, Nicholas P.; Matthews, Keith] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
   [Bogosavljevic, Milan] Astron Observ, Belgrade 11060, Serbia.
   [Shapley, Alice E.; Nestor, Daniel B.; Mace, Gregory; McLean, Ian S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
   [Kulas, Kristin R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Law, David R.; Rudie, Gwen C.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
   [Rudie, Gwen C.] Carnegie Observ, Pasadena, CA 91101 USA.
   [Reddy, Naveen A.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
   [Pettini, Max] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
RP Erb, DK (reprint author), Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, 1900 East Kenwood Blvd, Milwaukee, WI 53211 USA.
EM erbd@uwm.edu
FU US National Science Foundation [AST-1255591]; NSF [AST-0908805,
   AST-1313472]; NSF; Serbian MESTD [ON176021]; NSF "Telescope System
   Instrumentation Program" (TSIP)
FX We would like to thank the referee for a thoughtful and constructive
   report. D. K. E. is supported by the US National Science Foundation
   through the Faculty Early Career Development (CAREER) Program, grant
   AST-1255591. Additional support comes from the NSF through grants
   AST-0908805 (C. C. S., G. C. R., M. B.) and AST-1313472 (C. C. S., R. F.
   T., A. L. S.), and an NSF Graduate Student Research Fellowship (A. L.
   S.). M. B. acknowledges support of Serbian MESTD through grant ON176021.
   MOSFIRE was made possible by grants to WMKO from the NSF "Telescope
   System Instrumentation Program" (TSIP) and a generous donation from
   Gordon and Betty Moore. We thank our colleagues on the MOSFIRE
   instrument team, particularly Marcia Brown, Khan Bui, John Cromer, Jason
   Fucik, Hector Rodriguez, Bob Weber, and Jeff Zolkower at Caltech; Ted
   Aliado, George Brims, John Canfield, Chris Johnson, Ken Magnone, and
   Jason Weiss at UCLA; Harland Epps at UCO/Lick Observatory; and Sean
   Adkins at WMKO. Special thanks to all of the WMKO staff who helped make
   MOSFIRE commissioning successful, especially Marc Kassis, Allan Honey,
   Greg Wirth, Shui Kwok, Liz Chock, and Jim Lyke. Finally, we wish to
   extend thanks to those of Hawaiian ancestry on whose sacred mountain we
   are privileged to be guests.
NR 88
TC 34
Z9 34
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 NOV 1
PY 2014
VL 795
IS 1
AR 33
DI 10.1088/0004-637X/795/1/33
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300033
ER

PT J
AU Eufrasio, RT
   Dwek, E
   Arendt, RG
   de Mello, DF
   Gadotti, DA
   Urrutia-Viscarra, F
   de Oliveira, CM
   Benford, DJ
AF Eufrasio, Rafael T.
   Dwek, Eli
   Arendt, Richard G.
   de Mello, Duilia F.
   Gadotti, Dimitri A.
   Urrutia-Viscarra, Fernanda
   de Oliveira, Claudia Mendes
   Benford, Dominic J.
TI STAR FORMATION HISTORIES ACROSS THE INTERACTING GALAXY NGC 6872, THE
   LARGEST-KNOWN SPIRAL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 6872, IC 4970); galaxies: interactions;
   galaxies: spiral; galaxies: star formation; galaxies: stellar content
ID DIGITAL SKY SURVEY; TIDAL DWARF GALAXY; STRUCTURAL-PROPERTIES; BARRED
   GALAXIES; FORMATION RATES; PAVO GROUP; NGC-6872; DUST; GAS;
   DECOMPOSITION
AB NGC6872, hereafter the Condor, is a large spiral galaxy that is interacting with its closest companion, the S0 galaxy IC 4970. The extent of the Condor provides an opportunity for detailed investigation of the impact of the interaction on the current star formation rate and its history across the galaxy, on the age and spatial distribution of its stellar population, and on the mechanism that drives the star formation activity. To address these issues we analyzed the far-ultraviolet (FUV) to near-infrared (near-IR) spectral energy distribution of seventeen 10 kpc diameter regions across the galaxy, and derived their star formation history, current star formation rate, and stellar population and mass. We find that most of the star formation takes place in the extended arms, with very little star formation in the central 5 kpc of the galaxy, in contrast to what was predicted from previous numerical simulations. There is a trend of increasing star formation activity with distance from the nucleus of the galaxy, and no evidence for a recent increase in the current star formation rate due to the interaction. The nucleus itself shows no significant current star formation activity. The extent of the Condor also provides an opportunity to test the applicability of a single standard prescription for conversion of the FUV + IR (22 mu m) intensities to a star formation rate for all regions. We find that the conversion factor differs from region to region, arising from regional differences in the stellar populations.
C1 [Eufrasio, Rafael T.; de Mello, Duilia F.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
   [Eufrasio, Rafael T.; Dwek, Eli; Arendt, Richard G.; de Mello, Duilia F.; Benford, Dominic J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
   [Arendt, Richard G.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
   [de Mello, Duilia F.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
   [Gadotti, Dimitri A.] European So Observ, Santiago 19, Chile.
   [Urrutia-Viscarra, Fernanda; de Oliveira, Claudia Mendes] Univ Sao Paulo, Dept Astron, Inst Astron Geofis & Ciencias Atmosfericas, BR-05508090 Sao Paulo, Brazil.
RP Eufrasio, RT (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
EM rafael.t.eufrasio@nasa.gov
RI Benford, Dominic/D-4760-2012; Eufrasio, Rafael/F-7611-2016; 
OI Benford, Dominic/0000-0002-9884-4206; Eufrasio,
   Rafael/0000-0002-2987-1796; Arendt, Richard/0000-0001-8403-8548
FU NASA ADAP [NNX09AC72G]; NASA [NAS5-98034]; National Aeronautics and
   Space Administration; National Science Foundation
FX We thank the anonymous referee for comments that significantly improved
   the paper. E. D. acknowledges NASA ADAP proposal NNH11ZDA001N and DFdM
   was funded by NASA ADAP NNX09AC72G. Based on observations made with the
   NASA Galaxy Evolution Explorer. GALEX is operated for NASA by the
   California Institute of Technology under NASA contract NAS5-98034. This
   publication makes use of data products from the 2MASS, which is a joint
   project of the University of Massachusetts and the Infrared Processing
   and Analysis Center/California Institute of Technology, funded by the
   National Aeronautics and Space Administration and the National Science
   Foundation. This work is based 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.
NR 47
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 NOV 1
PY 2014
VL 795
IS 1
AR 89
DI 10.1088/0004-637X/795/1/89
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300089
ER

PT J
AU Giacintucci, S
   Markevitch, M
   Brunetti, G
   ZuHone, JA
   Venturi, T
   Mazzotta, P
   Bourdin, H
AF Giacintucci, S.
   Markevitch, M.
   Brunetti, G.
   ZuHone, J. A.
   Venturi, T.
   Mazzotta, P.
   Bourdin, H.
TI MAPPING THE PARTICLE ACCELERATION IN THE COOL CORE OF THE GALAXY CLUSTER
   RX J1720.1+2638
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual (RX
   J1720.1+2638); galaxies: clusters: intracluster medium; radio continuum:
   galaxies; radio continuum: general; X-rays: galaxies: clusters
ID RADIO MINI-HALOS; COLD FRONTS; COSMIC-RAYS; SCALING RELATIONS; PERSEUS
   CLUSTER; CHANDRA; ORIGIN; EMISSION; GAS; TURBULENCE
AB We present new deep, high-resolution radio images of the diffuse minihalo in the cool core of the galaxy cluster RX J1720.1+2638. The images have been obtained with the Giant Metrewave Radio Telescope at 317, 617, and 1280 MHz and with the Very Large Array at 1.5, 4.9, and 8.4 GHz, with angular resolutions ranging from 1 '' to 10 ''. This represents the best radio spectral and imaging data set for any minihalo. Most of the radio flux of the minihalo arises from a bright central component with a maximum radius of similar to 80 kpc. A fainter tail of emission extends out from the central component to form a spiral-shaped structure with a length of similar to 230 kpc, seen at frequencies 1.5 GHz and below. We find indication of a possible steepening of the total radio spectrum of the minihalo at high frequencies. Furthermore, a spectral index image shows that the spectrum of the diffuse emission steepens with increasing distance along the tail. A striking spatial correlation is observed between the minihalo emission and two cold fronts visible in the Chandra X-ray image of this cool core. These cold fronts confine the minihalo, as also seen in numerical simulations of minihalo formation by sloshing-induced turbulence. All these observations favor the hypothesis that the radio-emitting electrons in cluster cool cores are produced by turbulent re-acceleration.
C1 [Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Giacintucci, S.; Markevitch, M.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
   [Markevitch, M.; ZuHone, J. A.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
   [Brunetti, G.; Venturi, T.] INAF Ist Radioastron, I-40129 Bologna, Italy.
   [Mazzotta, P.; Bourdin, H.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RP Giacintucci, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM simona@astro.umd.edu
RI Mazzotta, Pasquale/B-1225-2016; 
OI Mazzotta, Pasquale/0000-0002-5411-1748; Brunetti,
   Gianfranco/0000-0003-4195-8613; Venturi, Tiziana/0000-0002-8476-6307;
   Giacintucci, Simona/0000-0002-1634-9886
FU NASA through Einstein Postdoctoral Fellowship by Chandra X-ray Center
   (CXC) [PF0-110071]; NASA
FX The authors thank the anonymous referee, whose comments and suggestions
   improved the paper. S. G. thanks Tracy Clarke for useful discussions. S.
   G. acknowledges the support of NASA through Einstein Postdoctoral
   Fellowship PF0-110071 awarded by the Chandra X-ray Center (CXC), which
   is operated by SAO. J.A.Z. is supported by the NASA Postdoctoral
   Program. GMRT is run by the National Centre for Radio Astrophysics of
   the Tata Institute of Fundamental Research. The National Radio Astronomy
   Observatory is a facility of the National Science Foundation operated
   under cooperative agreement by Associated Universities, Inc. The
   scientific results reported in this article are based on observations
   made by the Chandra X-Ray Observatory.
NR 57
TC 11
Z9 11
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 NOV 1
PY 2014
VL 795
IS 1
AR 73
DI 10.1088/0004-637X/795/1/73
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300073
ER

PT J
AU Hariharan, K
   Ramesh, R
   Kishore, P
   Kathiravan, C
   Gopalswamy, N
AF Hariharan, K.
   Ramesh, R.
   Kishore, P.
   Kathiravan, C.
   Gopalswamy, N.
TI AN ESTIMATE OF THE CORONAL MAGNETIC FIELD NEAR A SOLAR CORONAL MASS
   EJECTION FROM LOW-FREQUENCY RADIO OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE solar-terrestrial relations; Sun: activity; Sun: corona; Sun: coronal
   mass ejections (CMEs); Sun: magnetic fields; Sun: radio radiation
ID 1973 JANUARY 11; 9 R PERIOD; II BURSTS; GAURIBIDANUR RADIOHELIOGRAPH;
   INTERPLANETARY SHOCKS; VLA OBSERVATIONS; PLASMA EMISSION; ACTIVE
   REGIONS; QUIET SUN; POLARIZATION
AB We report ground-based, low-frequency (<100 MHz) radio imaging, spectral, and polarimeter observations of the type II radio burst associated with the solar coronal mass ejection (CME) that occurred on 2013 May 2. The spectral observations indicate that the burst has fundamental (F) and harmonic (H) emission components with split-band and herringbone structures. The imaging observations at 80 MHz indicate that the H component of the burst was located close to leading edge of the CME at a radial distance of r approximate to 2 R-circle dot in the solar atmosphere. The polarimeter observations of the type II burst, also at 80 MHz, indicate that the peak degree of circular polarization (dcp) corresponding to the emission generated in the corona ahead of and behind the associated MHD shock front are approximate to 0.05 +/- 0.02 and approximate to 0.1 +/- 0.01, respectively. We calculated the magnetic field B in the above two coronal regions by adopting the empirical relationship between the dcp and B for the harmonic plasma emission and the values are approximate to(0.7-1.4) +/- 0.2 G and approximate to(1.4-2.8) +/- 0.1 G, respectively.
C1 [Hariharan, K.; Ramesh, R.; Kishore, P.; Kathiravan, C.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
   [Gopalswamy, N.] NASA, Solar Phys Lab, GSFC, Greenbelt, MD USA.
RP Hariharan, K (reprint author), Indian Inst Astrophys, 2 Block, Bangalore 560034, Karnataka, India.
EM khariharan@iiap.res.in
OI Gopalswamy, Nat/0000-0001-5894-9954
NR 89
TC 6
Z9 6
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 NOV 1
PY 2014
VL 795
IS 1
AR 14
DI 10.1088/0004-637X/795/1/14
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300014
ER

PT J
AU Horch, EP
   Howell, SB
   Everett, ME
   Ciardi, DR
AF Horch, Elliott P.
   Howell, Steve B.
   Everett, Mark E.
   Ciardi, David R.
TI MOST SUB-ARCSECOND COMPANIONS OF KEPLER EXOPLANET CANDIDATE HOST STARS
   ARE GRAVITATIONALLY BOUND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: visual; planetary systems; stars: solar-type; techniques: high
   angular resolution; techniques: interferometric; techniques: photometric
ID SOLAR-TYPE STARS; BINARY STARS; STELLAR MULTIPLICITY; PLANET CANDIDATES;
   HIPPARCOS STARS; SYSTEMS; VALIDATION; AU; SAMPLE
AB Using the known detection limits for high-resolution imaging observations and the statistical properties of true binary and line-of-sight companions, we estimate the binary fraction of Kepler exoplanet host stars. Our speckle imaging programs at the WIYN 3.5 m and Gemini North 8.1 m telescopes have observed over 600 Kepler objects of interest and detected 49 stellar companions within similar to 1 arcsec. Assuming binary stars follow a log-normal period distribution for an effective temperature range of 3000-10,000 K, then the model predicts that the vast majority of detected sub-arcsecond companions are long period (P > 50 yr), gravitationally bound companions. In comparing the model predictions to the number of real detections in both observational programs, we conclude that the overall binary fraction of host stars is similar to the 40%-50% rate observed for field stars.
C1 [Horch, Elliott P.] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
   [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
   [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Horch, EP (reprint author), Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA.
EM horche2@southernct.edu; steve.b.howell@nasa.gov; everett@noao.edu;
   ciardi@ipac.caltech.edu
OI Ciardi, David/0000-0002-5741-3047
FU Kepler Project Office at the NASA Ames Research Center; Kepler Project
   Office
FX We thank the Kepler Project Office located at the NASA Ames Research
   Center for providing partial financial support for the upgraded DSSI
   instrument. It is also a pleasure to thank Steve Hardash, Andy Adamson,
   Inger Jorgensen, and the entire summit crew for their assistance at
   Gemini, as well as Charles Corson and the team of observing assistants
   at WIYN for all of their help during our runs over the last few years.
   We also thank the anonymous referee for her/his comments that have
   helped to significantly improve the paper. This work was funded by the
   Kepler Project Office.
NR 29
TC 34
Z9 34
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 NOV 1
PY 2014
VL 795
IS 1
AR 60
DI 10.1088/0004-637X/795/1/60
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300060
ER

PT J
AU Kipping, DM
   Torres, G
   Buchhave, LA
   Kenyon, SJ
   Henze, C
   Isaacson, H
   Kolbl, R
   Marcy, GW
   Bryson, ST
   Stassun, K
   Bastien, F
AF Kipping, D. M.
   Torres, G.
   Buchhave, L. A.
   Kenyon, S. J.
   Henze, C.
   Isaacson, H.
   Kolbl, R.
   Marcy, G. W.
   Bryson, S. T.
   Stassun, K.
   Bastien, F.
TI DISCOVERY OF A TRANSITING PLANET NEAR THE SNOW-LINE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planets and satellites: detection; stars: individual
   (KOI-1274); techniques: photometric
ID GAS GIANT PLANETS; EARTH-SIZED PLANETS; SUN-LIKE STARS; EXTRASOLAR
   PLANETS; HABITABLE-ZONE; INTERSTELLAR EXTINCTION; PHOTOMETRIC SURVEY;
   INFRARED-EMISSION; FALSE POSITIVES; BLEND SCENARIOS
AB In most theories of planet formation, the snow-line represents a boundary between the emergence of the interior rocky planets and the exterior ice giants. The wide separation of the snow-line makes the discovery of transiting worlds challenging, yet transits would allow for detailed subsequent characterization. We present the discovery of Kepler-421b, a Uranus-sized exoplanet transiting a G9/K0 dwarf once every 704.2 days in a near-circular orbit. Using public Kepler photometry, we demonstrate that the two observed transits can be uniquely attributed to the 704.2 day period. Detailed light curve analysis with BLENDER validates the planetary nature of Kepler-421b to >4 sigma confidence. Kepler-421b receives the same insolation as a body at similar to 2 AU in the solar system, as well as a Uranian albedo, which would have an effective temperature of similar to 180 K. Using a time-dependent model for the protoplanetary disk, we estimate that Kepler-421b's present semi-major axis was beyond the snow-line after similar to 3 Myr, indicating that Kepler-421b may have formed at its observed location.
C1 [Kipping, D. M.; Torres, G.; Buchhave, L. A.; Kenyon, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Buchhave, L. A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
   [Henze, C.; Bryson, S. T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Isaacson, H.; Kolbl, R.; Marcy, G. W.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
   [Stassun, K.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
   [Stassun, K.; Bastien, F.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dkipping@cfa.harvard.edu
OI Kenyon, Scott/0000-0003-0214-609X; Buchhave, Lars A./0000-0003-1605-5666
FU NASA Carl Sagan Fellowships; NASA [NNX14AB83G]
FX This work made use of the Michael Dodds Computing Facility and the
   Pleiades supercomputer at NASA Ames. D. M. K. is funded by the NASA Carl
   Sagan Fellowships. G. T. acknowledges partial support for this work from
   NASA grant NNX14AB83G (Kepler Participating Scientist Program). We offer
   our thanks and praise to the extraordinary scientists, engineers, and
   individuals who have made the Kepler Mission possible. We also thank C.
   Burke and J. Twicken for assistance in obtaining the centroid motion
   results.
NR 105
TC 13
Z9 13
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 NOV 1
PY 2014
VL 795
IS 1
AR 25
DI 10.1088/0004-637X/795/1/25
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300025
ER

PT J
AU Orr, ME
   Pineda, JL
   Goldsmith, PF
AF Orr, Matthew E.
   Pineda, Jorge L.
   Goldsmith, Paul F.
TI PHOTON-DOMINATED REGION MODELING OF THE [CI], [CII], AND CO LINE
   EMISSION FROM A BOUNDARY IN THE TAURUS MOLECULAR CLOUD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; infrared: ISM; ISM: individual objects (Taurus); line:
   profiles; methods: numerical; photon-dominated region (PDR)
ID C-12/C-13 ISOTOPE RATIO; NARROW SELF-ABSORPTION; INTERSTELLAR-MEDIUM;
   STAR-FORMATION; DARK CLOUDS; GAS; DENSITY; CARBON; DUST; RECOMBINATION
AB We present [CI] and [CII] observations of a linear edge region in the Taurus molecular cloud, and model this region as a cylindrically symmetric photon-dominated region (PDR) exposed to a low-intensity UV radiation field. The sharp, long profile of the linear edge makes it an ideal case to test PDR models and determine cloud parameters. We compare observations of the [C I], P-3(1) -> P-3(0) (492 GHz), [CI] P-3(2) -> P-3(1) (809 GHz), and [CII] P-2(3/2) -> P-2(1/2) (1900 GHz) transitions, as well as the lowest rotational transitions of (CO)-C-12 and (CO)-C-13, with line intensities produced by the RATRAN radiative transfer code from the results of the Meudon PDR code. We constrain the density structure of the cloud by fitting a cylindrical density function to visual extinction data. We study the effects of variation of the FUV field, C-12/C-13 isotopic abundance ratio, sulfur depletion, cosmic ray ionization rate, and inclination of the filament relative to the sky-plane on the chemical network of the PDR model and resulting line emission. We also consider the role of suprathermal chemistry and density inhomogeneities. We find good agreement between the model and observations, and that the integrated line intensities can be explained by a PDR model with an external FUV field of 0.05 G(0), a low ratio of C-12 to C-13 similar to 43, a highly depleted sulfur abundance (by a factor of at least 50), a cosmic ray ionization rate (3-6) x 10(-17) s(-1), and without significant effects from inclination, clumping or suprathermal chemistry.
C1 [Orr, Matthew E.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA.
   [Orr, Matthew E.; Pineda, Jorge L.; Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Orr, ME (reprint author), Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA.
RI Goldsmith, Paul/H-3159-2016; 
OI Orr, Matthew/0000-0003-1053-3081
NR 49
TC 6
Z9 6
U1 0
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 NOV 1
PY 2014
VL 795
IS 1
AR 26
DI 10.1088/0004-637X/795/1/26
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300026
ER

PT J
AU Pei, LY
   Barth, AJ
   Aldering, GS
   Briley, MM
   Carroll, CJ
   Carson, DJ
   Cenko, SB
   Clubb, KI
   Cohen, DP
   Cucchiara, A
   Desjardins, TD
   Edelson, R
   Fang, JJ
   Fedrow, JM
   Filippenko, AV
   Fox, OD
   Furniss, A
   Gates, EL
   Gregg, M
   Gustafson, S
   Horst, JC
   Joner, MD
   Kelly, PL
   Lacy, M
   Laney, CD
   Leonard, DC
   Li, WD
   Malkan, MA
   Margon, B
   Neeleman, M
   Nguyen, ML
   Prochaska, JX
   Ross, NR
   Sand, DJ
   Searcy, KJ
   Shivvers, IS
   Silverman, JM
   Smith, GH
   Suzuki, N
   Smith, KL
   Tytler, D
   Werk, JK
   Worseck, G
AF Pei, Liuyi
   Barth, Aaron J.
   Aldering, Greg S.
   Briley, Michael M.
   Carroll, Carla J.
   Carson, Daniel J.
   Cenko, S. Bradley
   Clubb, Kelsey I.
   Cohen, Daniel P.
   Cucchiara, Antonino
   Desjardins, Tyler D.
   Edelson, Rick
   Fang, Jerome J.
   Fedrow, Joseph M.
   Filippenko, Alexei V.
   Fox, Ori D.
   Furniss, Amy
   Gates, Elinor L.
   Gregg, Michael
   Gustafson, Scott
   Horst, J. Chuck
   Joner, Michael D.
   Kelly, Patrick L.
   Lacy, Mark
   Laney, C. David
   Leonard, Douglas C.
   Li, Weidong
   Malkan, Matthew A.
   Margon, Bruce
   Neeleman, Marcel
   Nguyen, My L.
   Prochaska, J. Xavier
   Ross, Nathaniel R.
   Sand, David J.
   Searcy, Kinchen J.
   Shivvers, Isaac S.
   Silverman, Jeffrey M.
   Smith, Graeme H.
   Suzuki, Nao
   Smith, Krista Lynne
   Tytler, David
   Werk, Jessica K.
   Worseck, Gabor
TI REVERBERATION MAPPING OF THE KEPLER FIELD AGN KA1858+4850
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (1RXSJ185800.9+485020); galaxies:
   nuclei
ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; BLACK-HOLE MASS; RAPID
   OPTICAL VARIABILITY; MONITORING PROJECT; LUMINOSITY RELATIONSHIP;
   RECOMBINATION LINES; QUASARS; GALAXIES; CALIBRATION
AB KA1858+4850 is a narrow-line Seyfert 1 galaxy at redshift 0.078 and is among the brightest active galaxies monitored by the Kepler mission. We have carried out a reverberation mapping campaign designed to measure the broad-line region size and estimate the mass of the black hole in this galaxy. We obtained 74 epochs of spectroscopic data using the Kast Spectrograph at the Lick 3 m telescope from 2012 February to November, and obtained complementary V-band images from five other ground-based telescopes. We measured the H beta light curve lag with respect to the V-band continuum light curve using both cross-correlation techniques (CCF) and continuum light curve variability modeling with the JAVELIN method and found rest-frame lags of tau(CCF) = 13.53(+2.03)(-2.32) days and tau(JAVELIN) = 13.15(+1.08)(-1.00) days. The H beta rms line profile has a width of sigma line = 770 +/- 49 km s(-1). Combining these two results and assuming a virial scale factor of f = 5.13, we obtained a virial estimate of M-BH = 8.06(+1.59)(-1.72) x 10(6) M circle dot for the mass of the central black hole and an Eddington ratio of L/L-Edd approximate to 0.2. We also obtained consistent but slightly shorter emission-line lags with respect to the Kepler light curve. Thanks to the Kepler mission, the light curve of KA1858+4850 has among the highest cadences and signal-to-noise ratios ever measured for an active galactic nucleus; thus, our black hole mass measurement will serve as a reference point for relations between black hole mass and continuum variability characteristics in active galactic nuclei.
C1 [Pei, Liuyi; Barth, Aaron J.; Carson, Daniel J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
   [Aldering, Greg S.; Cucchiara, Antonino] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
   [Briley, Michael M.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA.
   [Carroll, Carla J.; Joner, Michael D.; Laney, C. David] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA.
   [Cenko, S. Bradley; Edelson, Rick; Smith, Krista Lynne] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Cenko, S. Bradley] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
   [Clubb, Kelsey I.; Cohen, Daniel P.; Cucchiara, Antonino; Filippenko, Alexei V.; Fox, Ori D.; Kelly, Patrick L.; Li, Weidong; Shivvers, Isaac S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Desjardins, Tyler D.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
   [Fang, Jerome J.; Margon, Bruce; Prochaska, J. Xavier; Werk, Jessica K.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Fedrow, Joseph M.; Horst, J. Chuck; Leonard, Douglas C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
   [Fedrow, Joseph M.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
   [Furniss, Amy] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
   [Gates, Elinor L.] Univ Calif Santa Cruz, Lick Observ, Mt Hamilton, CA 95140 USA.
   [Gregg, Michael] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
   [Gustafson, Scott; Neeleman, Marcel; Tytler, David] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
   [Lacy, Mark] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
   [Malkan, Matthew A.; Ross, Nathaniel R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
   [Nguyen, My L.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
   [Prochaska, J. Xavier; Smith, Graeme H.; Werk, Jessica K.; Worseck, Gabor] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
   [Sand, David J.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
   [Sand, David J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
   [Searcy, Kinchen J.] San Diego Astron Assoc, San Diego, CA 92193 USA.
   [Silverman, Jeffrey M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
   [Suzuki, Nao] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
RP Pei, LY (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
OI Worseck, Gabor/0000-0003-0960-3580; Shivvers, Isaac/0000-0003-3373-8047;
   Barth, Aaron/0000-0002-3026-0562
FU NSF [AST-1108835, AST-1107812, AST-1108665, AST-1211916, AST-1302771,
   AST-1009571, AST-1210311, AST-0618209]; TABASGO Foundation; Christopher
   R. Redlich Fund; NASA [NAS5-26555]; NASA Office of Space Science
   [NNX13AC07G]; NASA Science Mission directorate
FX Research by L. P. and A.J.B. at UC Irvine has been supported by NSF
   grant AST-1108835. Research by M. A. M. at UCLA was supported by NSF
   grant AST-1107812. A.V.F.'s group at UC Berkeley was supported through
   NSF grants AST-1108665 and AST-1211916, the TABASGO Foundation, and the
   Christopher R. Redlich Fund. KAIT and its ongoing operation were made
   possible by donations from Sun Microsystems, Inc., the Hewlett-Packard
   Company, AutoScope Corporation, Lick Observatory, the NSF, the
   University of California, the Sylvia & Jim Katzman Foundation, and the
   TABASGO Foundation. We are very grateful to our late colleague Weidong
   Li, who was instrumental in making KAIT successful and taught us much
   about photometry.; J.M.S. is supported by an NSF Astronomy and
   Astrophysics Postdoctoral Fellowship under award AST-1302771. Research
   by D.C.L., J.C.H., and J.M.F. at San Diego State University is supported
   by NSF grants AST-1009571 and AST-1210311. The WMO 0.9 m telescope was
   funded by NSF grant AST-0618209.; This work makes use of observations
   from the LCOGT network. 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 paper includes data collected by the
   Kepler mission. Funding for the Kepler mission is provided by the NASA
   Science Mission directorate.
NR 58
TC 9
Z9 9
U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 1
PY 2014
VL 795
IS 1
AR 38
DI 10.1088/0004-637X/795/1/38
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300038
ER

PT J
AU Sharon, K
   Gladders, MD
   Rigby, JR
   Wuyts, E
   Bayliss, MB
   Johnson, TL
   Florian, MK
   Dahle, H
AF Sharon, Keren
   Gladders, Michael D.
   Rigby, Jane R.
   Wuyts, Eva
   Bayliss, Matthew B.
   Johnson, Traci L.
   Florian, Michael K.
   Dahle, Hakon
TI THE MASS DISTRIBUTION OF THE STRONG LENSING CLUSTER SDSS J1531+3414
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual (SDSS
   J1531+3414); gravitational lensing: strong
ID GIANT ARCS SURVEY; GALAXY CLUSTERS; RCSGA 032727-132609; LENSED
   GALAXIES; METALLICITY; CONSTRAINTS; CORES
AB We present the mass distribution at the core of SDSS J1531+3414, a strong-lensing cluster at z = 0.335. We find that the mass distribution is well described by two cluster-scale halos with a contribution from cluster-member galaxies. New Hubble Space Telescope observations of SDSS J1531+3414 reveal a signature of ongoing star formation associated with the two central galaxies at the core of the cluster, in the form of a chain of star forming regions at the center of the cluster. Using the lens model presented here, we place upper limits on the contribution of a possible lensed image to the flux at the central region, and rule out that this emission is coming from a background source.
C1 [Sharon, Keren; Johnson, Traci L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
   [Gladders, Michael D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
   [Gladders, Michael D.; Florian, Michael K.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
   [Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
   [Wuyts, Eva] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
   [Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
   [Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Dahle, Hakon] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
RP Sharon, K (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
EM kerens@umich.edu
FU NASA through a grant from the Space Telescope Science Institute
   [GO-13003]; NASA [NAS5-26555]
FX We wish to thank the anonymous referee for insightful comments. Support
   for program number GO-13003 was provided by NASA through a grant from
   the Space Telescope Science Institute, which is operated by the
   Association of Universities for Research in Astronomy, Inc., under NASA
   contract NAS5-26555. We also present results based on observations with
   the Nordic Optical Telescope, operated by the Nordic Optical Telescope
   Scientific Association at the Observatorio del Roque de los Muchachos,
   La Palma, Spain, of the Instituto de Astrofisica de Canarias.
NR 28
TC 10
Z9 10
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 NOV 1
PY 2014
VL 795
IS 1
AR 50
DI 10.1088/0004-637X/795/1/50
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300050
ER

PT J
AU Subramanian, S
   Tripathi, D
   Klimchuk, JA
   Mason, HE
AF Subramanian, Srividya
   Tripathi, Durgesh
   Klimchuk, James A.
   Mason, Helen E.
TI EMISSION MEASURE DISTRIBUTION FOR DIFFUSE REGIONS IN SOLAR ACTIVE
   REGIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: observational; Sun: abundances; Sun: atmosphere; Sun: corona;
   Sun: transition region; Sun: UV radiation; techniques: spectroscopic
ID ULTRAVIOLET IMAGING SPECTROMETER; TRANSITION-REGION; CORONAL-EXPLORER;
   TIME-DEPENDENCE; DOPPLER SHIFTS; LOOPS; CORE; DIAGNOSTICS; HINODE/EIS;
   ATMOSPHERE
AB Our knowledge of the diffuse emission that encompasses active regions is very limited. In this paper we investigate two off-limb active regions, namely, AR 10939 and AR 10961, to probe the underlying heating mechanisms. For this purpose, we have used spectral observations from Hinode/EIS and employed the emission measure (EM) technique to obtain the thermal structure of these diffuse regions. Our results show that the characteristic EM distributions of the diffuse emission regions peak at log T = 6.25 and the coolward slopes are in the range 1.4-3.3. This suggests that both low-as well as high-frequency nanoflare heating events are at work. Our results provide additional constraints on the properties of these diffuse emission regions and their contribution to the background/foreground when active region cores are observed on-disk.
C1 [Subramanian, Srividya; Tripathi, Durgesh] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
   [Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Mason, Helen E.] Univ Cambridge, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England.
RP Subramanian, S (reprint author), Interuniv Ctr Astron & Astrophys, Post Bag 4, Pune 411007, Maharashtra, India.
RI Tripathi, Durgesh/D-9390-2012; Klimchuk, James/D-1041-2012
OI Tripathi, Durgesh/0000-0003-1689-6254; Klimchuk,
   James/0000-0003-2255-0305
FU NASA
FX Hinode is a Japanese mission developed and launched by ISAS/JAXA,
   collaborating with NAOJ as a domestic partner, and NASA and STFC (UK) as
   international partners. Scientific operation of the Hinode mission is
   conducted by the Hinode science team organized at ISAS/JAXA. This team
   mainly consists of scientists from institutes in the partner countries.
   Support for the post-launch operation is provided by JAXA and NAOJ
   (Japan), STFC (UK), NASA, ESA, and NSC (Norway). CHIANTI is a
   collaborative project involving researchers at NRL (USA), RAL (UK), and
   the Universities of Cambridge (UK), George Mason (USA), and Florence
   (Italy). The work of J.A.K. was funded by the NASA Supporting Research
   Program. H. E. M. acknowledges S. T. F. C. We acknowledge useful
   discussions at the ISSI on Active Region Heating. We thank Dr. Peter
   Young for his valuable comments and discussions. We thank the anonymous
   referee for thoughtful comments and a careful reading.
NR 46
TC 6
Z9 6
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 NOV 1
PY 2014
VL 795
IS 1
AR 76
DI 10.1088/0004-637X/795/1/76
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300076
ER

PT J
AU Takami, M
   Hasegawa, Y
   Muto, T
   Gu, PG
   Dong, RB
   Karr, JL
   Hashimoto, J
   Kusakabe, N
   Chapillon, E
   Tang, YW
   Itoh, Y
   Carson, J
   Follette, KB
   Mayama, S
   Sitko, M
   Janson, M
   Grady, CA
   Kudo, T
   Akiyama, E
   Kwon, J
   Takahashi, Y
   Suenaga, T
   Abe, L
   Brandner, W
   Brandt, TD
   Currie, T
   Egner, SE
   Feldt, M
   Guyon, O
   Hayano, Y
   Hayashi, M
   Hayashi, S
   Henning, T
   Hodapp, KW
   Honda, M
   Ishii, M
   Iye, M
   Kandori, R
   Knapp, GR
   Kuzuhara, M
   McElwain, MW
   Matsuo, T
   Miyama, S
   Morino, JI
   Moro-Martin, A
   Nishimura, T
   Pyo, TS
   Serabyn, E
   Suto, H
   Suzuki, R
   Takato, N
   Terada, H
   Thalmann, C
   Tomono, D
   Turner, EL
   Wisniewski, JP
   Watanabe, M
   Yamada, T
   Takami, H
   Usuda, T
   Tamura, M
AF Takami, Michihiro
   Hasegawa, Yasuhiro
   Muto, Takayuki
   Gu, Pin-Gao
   Dong, Ruobing
   Karr, Jennifer L.
   Hashimoto, Jun
   Kusakabe, Nobuyuki
   Chapillon, Edwige
   Tang, Ya-Wen
   Itoh, Youchi
   Carson, Joseph
   Follette, Katherine B.
   Mayama, Satoshi
   Sitko, Michael
   Janson, Markus
   Grady, Carol A.
   Kudo, Tomoyuki
   Akiyama, Eiji
   Kwon, Jungmi
   Takahashi, Yasuhiro
   Suenaga, Takuya
   Abe, Lyu
   Brandner, Wolfgang
   Brandt, Timothy D.
   Currie, Thayne
   Egner, Sebastian E.
   Feldt, Markus
   Guyon, Olivier
   Hayano, Yutaka
   Hayashi, Masahiko
   Hayashi, Saeko
   Henning, Thomas
   Hodapp, Klaus W.
   Honda, Mitsuhiko
   Ishii, Miki
   Iye, Masanori
   Kandori, Ryo
   Knapp, Gillian R.
   Kuzuhara, Masayuki
   McElwain, Michael W.
   Matsuo, Taro
   Miyama, Shoken
   Morino, Jun-Ichi
   Moro-Martin, Amaya
   Nishimura, Tetsuo
   Pyo, Tae-Soo
   Serabyn, Eugene
   Suto, Hiroshi
   Suzuki, Ryuji
   Takato, Naruhisa
   Terada, Hiroshi
   Thalmann, Christian
   Tomono, Daigo
   Turner, Edwin L.
   Wisniewski, John P.
   Watanabe, Makoto
   Yamada, Toru
   Takami, Hideki
   Usuda, Tomonori
   Tamura, Motohide
TI SURFACE GEOMETRY OF PROTOPLANETARY DISKS INFERRED FROM NEAR-INFRARED
   IMAGING POLARIMETRY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE polarization; protoplanetary disks; stars: individual (SAO 206462, MWC
   758, 2MASS J16042165-2130284, PDS 70, MWC 480); stars: pre-main sequence
ID SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; T-TAURI STARS;
   POLARIZED SCATTERED-LIGHT; CIRCUMSTELLAR DISK; TRANSITIONAL DISK;
   HIGH-RESOLUTION; UPPER SCORPIUS; PDS 70; PROTOSTELLAR ENVELOPES
AB We present a new method of analysis for determining the surface geometry of five protoplanetary disks observed with near-infrared imaging polarimetry using Subaru-HiCIAO. Using as inputs the observed distribution of polarized intensity (PI), disk inclination, assumed properties for dust scattering, and other reasonable approximations, we calculate a differential equation to derive the surface geometry. This equation is numerically integrated along the distance from the star at a given position angle. We show that, using these approximations, the local maxima in the PI distribution of spiral arms (SAO 206462, MWC 758) and rings (2MASS J16042165-2130284, PDS 70) are associated with local concave-up structures on the disk surface. We also show that the observed presence of an inner gap in scattered light still allows the possibility of a disk surface that is parallel to the light path from the star, or a disk that is shadowed by structures in the inner radii. Our analysis for rings does not show the presence of a vertical inner wall as often assumed in studies of disks with an inner gap. Finally, we summarize the implications of spiral and ring structures as potential signatures of ongoing planet formation.
C1 [Takami, Michihiro; Hasegawa, Yasuhiro; Gu, Pin-Gao; Karr, Jennifer L.; Chapillon, Edwige; Tang, Ya-Wen] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
   [Muto, Takayuki] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan.
   [Dong, Ruobing] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Nucl Sci, Berkeley, CA 94720 USA.
   [Dong, Ruobing] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Hashimoto, Jun; Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
   [Kusakabe, Nobuyuki; Akiyama, Eiji; Kwon, Jungmi; Takahashi, Yasuhiro; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Kuzuhara, Masayuki; Miyama, Shoken; Morino, Jun-Ichi; Suto, Hiroshi; Suzuki, Ryuji; Takami, Hideki; Usuda, Tomonori; Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
   [Itoh, Youchi] Univ Hyogo, Nishi Harima Astron Observ, Ctr Astron, Sayo, Hyogo 6795313, Japan.
   [Carson, Joseph] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
   [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.
   [Sitko, Michael] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
   [Janson, Markus] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
   [Grady, Carol A.] Eureka Sci, Oakland, CA 96402 USA.
   [Grady, Carol A.; McElwain, Michael W.] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
   [Kudo, Tomoyuki; Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo] Subaru Telescope, Hilo, HI 96720 USA.
   [Takahashi, Yasuhiro; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
   [Suenaga, Takuya; Tamura, Motohide] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
   [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.
   [Brandt, Timothy D.; Knapp, Gillian R.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
   [Currie, Thayne] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
   [Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
   [Honda, Mitsuhiko] Kanagawa Univ, Fac Sci, Dept Math & Phys, Hiratsuka, Kanagawa 2591293, Japan.
   [Kuzuhara, Masayuki] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan.
   [Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
   [Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
   [Moro-Martin, Amaya] CAB CSIC INTA, Dept Astrophys, E-28850 Madrid, Spain.
   [Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Thalmann, Christian] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
   [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 Takami, M (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
EM hiro@asiaa.sinica.edu.tw
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
FU Ministry of Science and Technology (MoST) of Taiwan
   [100-2112-M-001-007-MY3, 103-2112-M-001-029]; EACOA by East Asia Core
   Observatories Association; National Astronomical Observatory of Japan;
   National Astronomical Observatory of China; Korea Astronomy and Space
   Science Institute; JSPS KAKENHI [26800106, 23103004, 26400224]; NASA
   through Hubble Fellowship by Space Telescope Science Institute
   [HST-HF-51320.01-A]; NASA [NAS 5-26555]; JSPS [PD: 24.110]; NSF-AST
   [1009203, 1009314]; NSF [AST 1008440]
FX We are grateful for anonymous referees who provided thorough reviews and
   valuable comments. We thank the Subaru Telescope staff for their
   support, especially from Michael Lemmen for making our observations
   successful. We thank Dr. Hyosun Kim for useful discussion. M. T. is
   supported by the Ministry of Science and Technology (MoST) of Taiwan
   (Grant Nos. 100-2112-M-001-007-MY3 and 103-2112-M-001-029). Y.H. is
   supported by the EACOA Fellowship that is supported by the East Asia
   Core Observatories Association which consists of the Academia Sinica
   Institute of Astronomy and Astrophysics, the National Astronomical
   Observatory of Japan, the National Astronomical Observatory of China,
   and the Korea Astronomy and Space Science Institute. T. M. is supported
   by JSPS KAKENHI grant Nos. 26800106, 23103004, 26400224. R. D.
   acknowledges the support for this work by NASA through Hubble Fellowship
   grant HST-HF-51320.01-A awarded by the Space Telescope Science
   Institute, which is operated by the Association of Universities for
   Research in Astronomy, Inc., for NASA, under contract NAS 5-26555.
   Jungmi Kwon is supported by the JSPS Research Fellowships for Young
   Scientists (PD: 24.110). J.C. was supported by NSF-AST 1009203. C. A. G.
   acknowledges support under NSF AST 1008440. J.P.W. is supported by
   NSF-AST 1009314. This research made use of the Simbad data base operated
   at CDS, Strasbourg, France, and the NASA's Astrophysics Data System
   Abstract Service.
NR 77
TC 16
Z9 16
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 NOV 1
PY 2014
VL 795
IS 1
AR 71
DI 10.1088/0004-637X/795/1/71
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300071
ER

PT J
AU Uritsky, VM
   Davila, JM
AF Uritsky, Vadim M.
   Davila, Joseph M.
TI SPATIOTEMPORAL ORGANIZATION OF ENERGY RELEASE EVENTS IN THE QUIET SOLAR
   CORONA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instabilities; Sun: activity; Sun: corona; Sun: flares; Sun: magnetic
   fields
ID WAITING-TIME DISTRIBUTION; STRANGE ATTRACTORS; MAGNETIC-FIELD; FLARES;
   MODEL; CRITICALITY; STATISTICS; DYNAMICS; LOOPS; SUPERGRANULATION
AB Using data from the STEREO and SOHO spacecraft, we show that temporal organization of energy release events in the quiet solar corona is close to random, in contrast to the clustered behavior of flaring times in solar active regions. The locations of the quiet-Sun events follow the meso-and supergranulation pattern of the underling photosphere. Together with earlier reports of the scale-free event size statistics, our findings suggest that quiet solar regions responsible for bulk coronal heating operate in a driven self-organized critical state, possibly involving long-range Alfvenic interactions.
C1 [Uritsky, Vadim M.] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Davila, Joseph M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Uritsky, VM (reprint author), Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM vadim.uritsky@nasa.gov
FU NASA [NNG11PL10A 670.002]
FX We acknowledge J. Klimchuk, A. Pulkkinen, and J. Guerra for helpful
   discussions and A. Coyner for preparing solar images. The work of V. U.
   was supported by NASA grant NNG11PL10A 670.002 to CUA/IACS.
NR 49
TC 3
Z9 3
U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 1
PY 2014
VL 795
IS 1
AR 15
DI 10.1088/0004-637X/795/1/15
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8YN
UT WOS:000343857300015
ER

PT J
AU Aragao, LEOC
   Poulter, B
   Barlow, JB
   Anderson, LO
   Malhi, Y
   Saatchi, S
   Phillips, OL
   Gloor, E
AF Aragao, Luiz E. O. C.
   Poulter, Benjamin
   Barlow, Jos B.
   Anderson, Liana O.
   Malhi, Yadvinder
   Saatchi, Sassan
   Phillips, Oliver L.
   Gloor, Emanuel
TI Environmental change and the carbon balance of Amazonian forests
SO BIOLOGICAL REVIEWS
LA English
DT Review
DE carbon emissions; recovery; drought; fire; climate; secondary forests;
   deforestation
ID NET PRIMARY PRODUCTION; BRAZILIAN AMAZON; TROPICAL FORESTS; RAIN-FOREST;
   CLIMATE-CHANGE; FIRE SUSCEPTIBILITY; POSITIVE FEEDBACKS; SECONDARY
   FORESTS; SPATIAL-PATTERNS; TREE MORTALITY
AB Extreme climatic events and land-use change are known to influence strongly the current carbon cycle of Amazonia, and have the potential to cause significant global climate impacts. This review intends to evaluate the effects of both climate and anthropogenic perturbations on the carbon balance of the Brazilian Amazon and to understand how they interact with each other. By analysing the outputs of the Intergovernmental Panel for Climate Change (IPCC) Assessment Report 4 (AR4) model ensemble, we demonstrate that Amazonian temperatures and water stress are both likely to increase over the 21st Century. Curbing deforestation in the Brazilian Amazon by 62% in 2010 relative to the 1990s mean decreased the Brazilian Amazon's deforestation contribution to global land use carbon emissions from 17% in the 1990s and early 2000s to 9% by 2010. Carbon sources in Amazonia are likely to be dominated by climatic impacts allied with forest fires (48.3% relative contribution) during extreme droughts. The current net carbon sink (net biome productivity, NBP) of +0.16 (ranging from +0.11 to +0.21) Pg C year(-1) in the Brazilian Amazon, equivalent to 13.3% of global carbon emissions from land-use change for 2008, can be negated or reversed during drought years [NBP = -0.06 (-0.31 to +0.01) Pg C year(-1)]. Therefore, reducing forest fires, in addition to reducing deforestation, would be an important measure for minimizing future emissions. Conversely, doubling the current area of secondary forests and avoiding additional removal of primary forests would help the Amazonian gross forest sink to offset approximately 42% of global land-use change emissions. We conclude that a few strategic environmental policy measures are likely to strengthen the Amazonian net carbon sink with global implications. Moreover, these actions could increase the resilience of the net carbon sink to future increases in drought frequency.
C1 [Aragao, Luiz E. O. C.] Geog Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4RJ, Devon, England.
   [Aragao, Luiz E. O. C.; Anderson, Liana O.] Natl Inst Space Res, Remote Sensing Div, BR-12227010 Sao Paulo, Brazil.
   [Poulter, Benjamin] CNRS, UVSQ, CEA, Lab Sci Climat & Environm, F-91190 Gif Sur Yvette, France.
   [Barlow, Jos B.] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England.
   [Barlow, Jos B.] Museu Paraense Emilio Goeldi, BR-66077830 Belem, Para, Brazil.
   [Anderson, Liana O.; Malhi, Yadvinder] Univ Oxford, Sch Geog & Environm, Oxford OX1 3QY, England.
   [Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Phillips, Oliver L.; Gloor, Emanuel] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
RP Aragao, LEOC (reprint author), Geog Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4RJ, Devon, England.
EM laragao@dsr.inpe.br
RI Phillips, Oliver/A-1523-2011; Barlow, Jos/E-7861-2014; 
OI Phillips, Oliver/0000-0002-8993-6168; Poulter,
   Benjamin/0000-0002-9493-8600
FU UK Natural Environment Research Council (NERC) [NE/F015356/2,
   NE/l018123/1]; CNPq; CAPES; FP7 Marie Curie Incoming International
   Fellowship [220546]; NERC [NE/G000816/1]; Instituto Nacional de Ciencia
   e Tecnologia - Biodiversidade e Uso da Terra na Amazonia [CNPq
   574008/2008-0]; Gordon and Betty Moore Foundation; European Research
   Council; NERC AMAZONICA grant [NE/F005806/1]
FX L.E.O.C.A. acknowledges the support of the UK Natural Environment
   Research Council (NERC) grants (NE/F015356/2 and NE/l018123/1), the CNPq
   and CAPES for the Science without Borders Program Fellowship. B. P.
   acknowledges the support of the FP7 Marie Curie Incoming International
   Fellowship (Grant Number 220546). J.B.B. acknowledges the support of
   NERC grant (NE/G000816/1), the Instituto Nacional de Ciencia e
   Tecnologia - Biodiversidade e Uso da Terra na Amazonia (CNPq
   574008/2008-0) and CNPq and CAPES for the Science without Borders
   Program Fellowship. O.P. and Y.M. thank the Gordon and Betty Moore
   Foundation for support of the RAINFOR project which contributed to this
   review. O.P. is supported by an Advanced Grant from the European
   Research Council. E. G. and L.O.A. acknowledges the support of the NERC
   AMAZONICA grant (NE/F005806/1).
NR 112
TC 40
Z9 40
U1 20
U2 174
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1464-7931
EI 1469-185X
J9 BIOL REV
JI Biol. Rev.
PD NOV
PY 2014
VL 89
IS 4
BP 913
EP 931
DI 10.1111/brv.12088
PG 19
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA AS0XC
UT WOS:000343998100009
PM 25324039
ER

PT J
AU Lang, C
   Makhija, D
   Doostan, A
   Maute, K
AF Lang, Christapher
   Makhija, David
   Doostan, Alireza
   Maute, Kurt
TI A simple and efficient preconditioning scheme for heaviside enriched
   XFEM
SO COMPUTATIONAL MECHANICS
LA English
DT Article
DE Level set method; Extended finite element method; Heaviside enrichment;
   Ill-condition; Preconditioner
ID FINITE-ELEMENT-METHOD; TOPOLOGY OPTIMIZATION; BOUNDARY-CONDITIONS; FEM;
   SOLIDIFICATION; SIMULATION; SOLIDS; FLOWS
AB The extended finite element method (XFEM) is an approach for solving problems with non-smooth solutions, which arise from geometric features such as cracks, holes, and material inclusions. In the XFEM, the approximate solution is locally enriched to capture the discontinuities without requiring a mesh which conforms to the geometric features. One drawback of the XFEM is that an ill-conditioned system of equations results when the ratio of volumes on either side of the interface in an element is small. Such interface configurations are often unavoidable, in particular for moving interface problems on fixed meshes. In general, the ill-conditioning reduces the performance of iterative linear solvers and impedes the convergence of solvers for nonlinear problems. This paper studies the XFEM with a Heaviside enrichment strategy for solving problems with stationary and moving material interfaces. A generalized formulation of the XFEM is combined with the level set method to implicitly define the embedded interface geometry. In order to avoid the ill-conditioning, a simple and efficient scheme based on a geometric preconditioner and constraining degrees of freedom to zero for small intersections is proposed. The geometric preconditioner is computed from the nodal basis functions, and therefore may be constructed prior to building the system of equations. This feature and the low-cost of constructing the preconditioning matrix makes it well suited for nonlinear problems with fixed and moving interfaces. It is shown by numerical examples that the proposed preconditioning scheme performs well for discontinuous problems and C-0-continuous problems with both the stabilized Lagrange and Nitsche methods for enforcing the continuity constraint at the interface. Numerical examples are presented which compare the condition number and solution error with and without the proposed preconditioning scheme. The results suggest that the proposed preconditioning scheme leads to condition numbers similar to that of a body-fitted mesh using the traditional finite element method without loss of solution accuracy.
C1 [Lang, Christapher] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23665 USA.
   [Makhija, David; Doostan, Alireza; Maute, Kurt] Univ Colorado, Boulder, CO 80309 USA.
RP Doostan, A (reprint author), Univ Colorado, Boulder, CO 80309 USA.
EM doostan@colorado.edu
FU NASA Fundamental Aeronautics Program Fixed Wing Project; National
   Science Foundation [CMMI-0729520, EFRI SEED-1038305]; U.S. Department of
   Energy Office of Science, Office of Advanced Scientific Computing
   Research [DE-SC0006402]
FX The first author acknowledges the support of the NASA Fundamental
   Aeronautics Program Fixed Wing Project, and the second and fourth
   authors acknowledges the support of the National Science Foundation
   under grants CMMI-0729520 and EFRI SEED-1038305. This material is based
   upon work of third author supported by the U.S. Department of Energy
   Office of Science, Office of Advanced Scientific Computing Research,
   under Award Number DE-SC0006402. The opinions and conclusions presented
   are those of the authors and do not necessarily reflect the views of the
   sponsoring organizations.
NR 38
TC 13
Z9 13
U1 3
U2 16
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0178-7675
EI 1432-0924
J9 COMPUT MECH
JI Comput. Mech.
PD NOV
PY 2014
VL 54
IS 5
BP 1357
EP 1374
DI 10.1007/s00466-014-1063-8
PG 18
WC Mathematics, Interdisciplinary Applications; Mechanics
SC Mathematics; Mechanics
GA AR9EJ
UT WOS:000343874700018
ER

PT J
AU Ma, XG
   Zheng, JG
   Goldstein, JC
   Zednik, S
   Fu, LY
   Duggan, B
   Aulenbach, SM
   West, P
   Tilmes, C
   Fox, P
AF Ma, Xiaogang
   Zheng, Jin Guang
   Goldstein, Justin C.
   Zednik, Stephan
   Fu, Linyun
   Duggan, Brian
   Aulenbach, Steven M.
   West, Patrick
   Tilmes, Curt
   Fox, Peter
TI Ontology engineering in provenance enablement for the National Climate
   Assessment
SO ENVIRONMENTAL MODELLING & SOFTWARE
LA English
DT Article
DE Provenance; Ontology engineering; Use cases; Global change; Semantic web
ID GLOBAL CHANGE INFORMATION; SEMANTIC WEB; SCIENCE; SYSTEM
AB The National Climate Assessment of the U.S. Global Change Research Program (USGCRP) analyzes and presents the impacts of climate change on the United States. The provenance information in the assessment is important because the assessment findings are of great public and academic concern and are used in policy and decision-making. By applying a use case-driven iterative methodology, we developed information models and ontology to represent the content structure of the recent National Climate Assessment draft report and its associated provenance information. We tested the ontology by using it in pilot systems serving information about instances of chapters, scientific findings, figures, tables, images, datasets, references, people, and organizations, etc. in the draft report, as well as interrelationships among those instances. The results successfully help users trace provenance in the draft report, such as finding all the journal articles from which a figure in the report was derived. The provenance information in our work was maintained in the context of the "Web of Data". In addition to the pilot systems we developed, other tools and services are also able to retrieve and utilize the provenance information. Our work is part of a Global Change Information System coordinated by the USGCRP that will eventually cover provenance information for the entire scope of global change research. Such a system will greatly increase understanding, credibility and trust in the global change research and foster reproducibility of scientific results and conclusions. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Ma, Xiaogang; Zheng, Jin Guang; Zednik, Stephan; Fu, Linyun; West, Patrick; Fox, Peter] Rensselaer Polytech Inst, Tetherless World Constellat, Troy, NY 12180 USA.
   [Goldstein, Justin C.; Duggan, Brian; Aulenbach, Steven M.] Univ Corp Atmospher Res, Boulder, CO 80301 USA.
   [Goldstein, Justin C.; Duggan, Brian; Aulenbach, Steven M.; Tilmes, Curt] US Global Change Res Program, Washington, DC 20006 USA.
   [Tilmes, Curt] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ma, XG (reprint author), Rensselaer Polytech Inst, Tetherless World Constellat, 110 8th St, Troy, NY 12180 USA.
EM max7@rpi.edu
RI Goldstein, Justin/J-6880-2012; 
OI Goldstein, Justin/0000-0001-5414-9589; Duggan,
   Brian/0000-0001-5138-9130; Aulenbach, Steve/0000-0002-0172-6538; Zednik,
   Stephan/0000-0002-5635-9501; Ma, Xiaogang/0000-0002-9110-7369
FU National Science Foundation through the University Corporation for
   Atmospheric Research [S13-94358]
FX This paper is based on research funded by the National Science
   Foundation grant through the University Corporation for Atmospheric
   Research to RPI under contract S13-94358. The authors thank Tim Lebo and
   Deborah McGuinness for their comments on PROV-O, OPM and PML, and four
   anonymous reviewers for their detailed and constructive comments which
   led to the improvements in the manuscript.
NR 59
TC 6
Z9 6
U1 1
U2 10
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1364-8152
EI 1873-6726
J9 ENVIRON MODELL SOFTW
JI Environ. Modell. Softw.
PD NOV
PY 2014
VL 61
BP 191
EP 205
DI 10.1016/j.envsoft.2014.08.002
PG 15
WC Computer Science, Interdisciplinary Applications; Engineering,
   Environmental; Environmental Sciences
SC Computer Science; Engineering; Environmental Sciences & Ecology
GA AR8WP
UT WOS:000343852500016
ER

PT J
AU Rozas, LP
   Minello, TJ
   Miles, MS
AF Rozas, Lawrence P.
   Minello, Thomas J.
   Miles, M. Scott
TI Effect of Deepwater Horizon Oil on Growth Rates of Juvenile Penaeid
   Shrimps
SO ESTUARIES AND COASTS
LA English
DT Article
DE Field experiment; Growth comparison; Farfantepenaeus aztecus;
   Litopenaeus setiferus; Food addition
ID MARSH-EDGE FISHES; SALT-MARSH; WHITE SHRIMP; BROWN SHRIMP;
   PETROLEUM-HYDROCARBONS; AROMATIC-HYDROCARBONS; LITOPENAEUS-SETIFERUS;
   SOURCE IDENTIFICATION; GALVESTON-BAY; CRUDE-OIL
AB Marsh shoreline, an important habitat for juvenile penaeid shrimps, was extensively oiled in coastal Louisiana by the Deepwater Horizon oil spill of 2010. The effect of this spill on growth was examined for brown shrimp Farfantepenaeus aztecus and white shrimp Litopenaeus setiferus held for 7 days in field mesocosms in Barataria Bay during May and August 2011, respectively. The experiments each had 10 treatment combinations, five apparent oil levels, each one with and without added food. Mesocosms were placed in northern Barataria Bay along shorelines that varied in oiling (designated as heavy, moderate, light, very light, or none based on NOAA surveys), and shrimp in half the mesocosms received additional food. Polycyclic aromatic hydrocarbon (PAH) concentrations determined from sediment cores collected at each mesocosm were significantly higher at heavy and moderate than very light shorelines and also higher at moderate than light and none shorelines. Brown shrimp grew more slowly at heavy than very light or none shorelines, and a statistically significant negative relationship was detected between brown shrimp growth rates and sediment PAH concentrations. In August, PAH sediment concentrations had decreased significantly from the values measured in May, no significant difference in white shrimp growth rates was detected among oiling levels, and no relationship was detected between white shrimp growth and sediment PAH concentrations. Both brown shrimp and white shrimp grew more rapidly in mesocosms where food was added. Our study shows that exposure to nonlethal concentrations of petroleum hydrocarbons can reduce growth rates of juvenile penaeid shrimps.
C1 [Rozas, Lawrence P.] NOAA, Estuarine Habitats & Coastal Fisheries Ctr, Natl Marine Fisheries Serv, SEFSC, Lafayette, LA 70506 USA.
   [Minello, Thomas J.] NOAA, Galveston Lab, Natl Marine Fisheries Serv, SEFSC, Galveston, TX 77551 USA.
   [Miles, M. Scott] Louisiana State Univ, Dept Environm Sci, Baton Rouge, LA 70803 USA.
RP Rozas, LP (reprint author), NOAA, Estuarine Habitats & Coastal Fisheries Ctr, Natl Marine Fisheries Serv, SEFSC, 646 Cajundome Blvd, Lafayette, LA 70506 USA.
EM Lawrence.Rozas@noaa.gov
FU NOAA; Southeast Fisheries Science Center
FX This research was conducted through the NOAA National Marine Fisheries
   Service Southeast Fisheries Science Center by personnel from the Fishery
   Ecology Branch (FEB) located at the Galveston Laboratory and the
   Estuarine Habitats and Coastal Fisheries Center in Lafayette, LA. NOAA
   supplemental funding made available to examine impacts of the Deepwater
   Horizon spill supported this project. The assistance of everyone in the
   FEB was essential for the successful completion of this project. In
   particular, we thank Lainey Broussard, Harmon Brown, Kim Clausen, Jim
   Ditty, Jennifer Doerr, Shawn Hillen, Christin Hutchison, Trey Mace,
   Michael Prewitt, Vanessa Retzlaff, Juan Salas, and Heather Seiler for
   helping to conduct the field experiments and collect and process the
   samples. We acknowledge Buffy A. Meyer and Dr. Heng Gao for conducting
   the hydrocarbon analyses and Phil Caldwell for producing Fig. 1. Dr.
   Shahrokh Rouhani (NewFields Co., LLC) provided advice on statistical
   analyses. Two anonymous reviewers and Judy Grassle provided helpful
   suggestions that improved the original manuscript. We acknowledge NOAA
   and the Southeast Fisheries Science Center for funding this research
   project. The findings and conclusions in this paper are those of the
   authors and do not necessarily represent the views of the NOAA National
   Marine Fisheries Service.
NR 57
TC 7
Z9 7
U1 2
U2 90
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 NOV
PY 2014
VL 37
IS 6
BP 1403
EP 1414
DI 10.1007/s12237-013-9766-1
PG 12
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA AR6WY
UT WOS:000343722700008
ER

PT J
AU Johnston, R
   Bacon, D
   Teodoro, LFA
   Nichol, RC
   Warren, MS
   Cress, C
AF Johnston, R.
   Bacon, D.
   Teodoro, L. F. A.
   Nichol, R. C.
   Warren, M. S.
   Cress, C.
TI Reconstructing the velocity field beyond the local universe
SO GENERAL RELATIVITY AND GRAVITATION
LA English
DT Article
DE Methods: data analysis, numerical, statistical; Galaxies: distances and
   redshifts; Cosmology: large-scale structure of universe
ID LARGE-SCALE STRUCTURE; DIGITAL SKY SURVEY; EARLY-TYPE GALAXIES; PECULIAR
   VELOCITY; TULLY-FISHER; FUNDAMENTAL PLANE; REDSHIFT DATA; WIENER
   RECONSTRUCTION; ELLIPTIC GALAXIES; DENSITY
AB We present a maximum probability approach to reconstructing spatial maps of the peculiar velocity field at redshifts z similar to 0.1, where the velocities have been measured from distance indicators (DI) such as D-n - sigma relations or Tully-Fisher. With the large statistical uncertainties associated with DIs, our reconstruction method aims to recover the underlying true peculiar velocity field by reducing these errors with the use of two physically motivated filtering prior terms. The first constructs an estimate of the velocity field derived from the galaxy over-density delta(g) and the second makes use of the matter linear density power spectrum P-k. Using N-body simulations we find, with an SDSS-like sample (N-gal similar to 33 per deg(2)), an average correlation coefficient value of r = 0.55 +/- 0.02 between our reconstructed velocity field and that of the true velocity field from the simulation. However, with a suitably high number density of galaxies from the next generation surveys (e. g. N-gal similar or equal to 140 per deg(2)) we can achieve an average r = 0.70 +/- 0.02 out to moderate redshifts z similar to 0.1. This will prove useful for future tests of gravity, as these relatively deep maps are complementary to weak lensing maps at the same redshift. LA-UR 12-24505.
C1 [Johnston, R.] Univ Western Cape, Dept Phys, Cape Town, South Africa.
   [Bacon, D.; Nichol, R. C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
   [Teodoro, L. F. A.] NASA, BAER Inst, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Warren, M. S.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA.
   [Cress, C.] Ctr High Performance Comp, ZA-7700 Cape Town, South Africa.
RP Johnston, R (reprint author), Univ Western Cape, Dept Phys, Cape Town, South Africa.
EM rwi.johnston@gmail.com
FU SKA-South Africa; National Research Foundation (NRF); UK Science and
   Technology Facilities Council [ST/H002774/1, ST/K0090X/1]; ICG, at the
   University of Portsmouth
FX We would like to extend special thanks to Enzo Branchini and Adi Nusser
   for stimulating discussions, their comments and reading several drafts
   of this paper. We also would like to thank Martin Hendry, Mat Smith,
   Andreas Faltenbacher, Roy Maartens, Daniele Bertacca, Rafal
   Szepietowski, Yong-Seon Song, Kazuya Koyama, Prina Patel, Emma Beynon,
   Robert Crittenden and Philip Marshall for useful discussions. RJ
   acknowledges the support of the SKA-South Africa and the National
   Research Foundation (NRF), as well as the hospitality of the Institute
   of Cosmology and Gravitation (ICG) at the University of Portsmouth where
   some of this work was carried out. DB and RN are supported by the UK
   Science and Technology Facilities Council (Grant Nos. ST/H002774/1 and
   ST/K0090X/1). The analysis was performed with the SCIAMA High
   Performance Computing cluster supported by the ICG, at the University of
   Portsmouth. We would like to thank the SCIAMA cluster administrator,
   Gary Burton, for all his help. Please contact the authors to request
   access to research materials discussed in this paper.
NR 58
TC 1
Z9 1
U1 0
U2 2
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0001-7701
EI 1572-9532
J9 GEN RELAT GRAVIT
JI Gen. Relativ. Gravit.
PD NOV
PY 2014
VL 46
IS 11
AR 1812
DI 10.1007/s10714-014-1812-1
PG 18
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
   & Fields
SC Astronomy & Astrophysics; Physics
GA AR9FT
UT WOS:000343879000005
ER

PT J
AU Houghton, J
   Fike, D
   Druschel, G
   Orphan, V
   Hoehler, TM
   Des Marais, DJ
AF Houghton, J.
   Fike, D.
   Druschel, G.
   Orphan, V.
   Hoehler, T. M.
   Des Marais, D. J.
TI Spatial variability in photosynthetic and heterotrophic activity drives
   localized delta C-13(org) fluctuations and carbonate precipitation in
   hypersaline microbial mats
SO GEOBIOLOGY
LA English
DT Article
ID SULFATE-REDUCING BACTERIA; PURPLE SULFUR BACTERIA; ISOTOPE
   FRACTIONATION; CYANOBACTERIAL MATS; GUERRERO NEGRO; COMMUNITY;
   SEDIMENTS; MARINE; OXYGEN; CYCLE
AB Modern laminated photosynthetic microbial mats are ideal environments to study how microbial activity creates and modifies carbon and sulfur isotopic signatures prior to lithification. Laminated microbial mats from a hypersaline lagoon (Guerrero Negro, Baja California, Mexico) maintained in a flume in a greenhouse at NASA Ames Research Center were sampled for C-13 of organic material and carbonate to assess the impact of carbon fixation (e.g., photosynthesis) and decomposition (e.g., bacterial respiration) on C-13 signatures. In the photic zone, the C-13(org) signature records a complex relationship between the activities of cyanobacteria under variable conditions of CO2 limitation with a significant contribution from green sulfur bacteria using the reductive TCA cycle for carbon fixation. Carbonate is present in some layers of the mat, associated with high concentrations of bacteriochlorophyll e (characteristic of green sulfur bacteria) and exhibits C-13 signatures similar to DIC in the overlying water column (-2.0 parts per thousand), with small but variable decreases consistent with localized heterotrophic activity from sulfate-reducing bacteria (SRB). Model results indicate respiration rates in the upper 12mm of the mat alter in situ pH and HCO3 concentrations to create both phototrophic CO2 limitation and carbonate supersaturation, leading to local precipitation of carbonate minerals. The measured activity of SRB with depth suggests they variably contribute to decomposition in the mat dependent on organic substrate concentrations. Millimeter-scale variability in the C-13(org) signature beneath the photic zone in the mat is a result of shifting dominance between cyanobacteria and green sulfur bacteria with the aggregate signature overprinted by heterotrophic reworking by SRB and methanogens. These observations highlight the impact of sedimentary microbial processes on C-13(org) signatures; these processes need to be considered when attempting to relate observed isotopic signatures in ancient sedimentary strata to conditions in the overlying water column at the time of deposition and associated inferences about carbon cycling.
C1 [Houghton, J.; Fike, D.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
   [Druschel, G.] Indiana Univ Purdue Univ, Dept Earth Sci, Indianapolis, IN 46202 USA.
   [Orphan, V.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
   [Hoehler, T. M.; Des Marais, D. J.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
RP Houghton, J (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
EM jhoughton@levee.wustl.edu
RI Orphan, Victoria/K-1002-2014; Fike, David/D-3634-2011
OI Orphan, Victoria/0000-0002-5374-6178; Fike, David/0000-0003-2848-0328
FU NSF [EAR-1124389, EAR-1123391, EAR-1304352, EAR-1261423]; Packard
   Fellowship; Hansewissenschaftskolleg Fellowship
FX We would like to thank NASA AMES NAI team, particularly Mike Kubo, Linda
   Jahnke, and Abigail Green-Saxena for discussion and assistance in the
   laboratory and field, and Exportadora del Sal, S. A. for access to the
   field site. Funding for this work was supported by NSF EAR-1124389 as
   well as a Packard Fellowship and a Hansewissenschaftskolleg Fellowship
   to D. A. F., NSF EAR-1123391 to V.J.O, and NSF EAR-1304352 and
   EAR-1261423 to G.D.
NR 75
TC 3
Z9 3
U1 1
U2 20
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1472-4677
EI 1472-4669
J9 GEOBIOLOGY
JI Geobiology
PD NOV
PY 2014
VL 12
IS 6
BP 557
EP 574
DI 10.1111/gbi.12113
PG 18
WC Biology; Environmental Sciences; Geosciences, Multidisciplinary
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
   Ecology; Geology
GA AR9BR
UT WOS:000343866600006
PM 25312537
ER

PT J
AU Johnson, PV
   Hodyss, R
   Beauchamp, JL
AF Johnson, Paul V.
   Hodyss, Robert
   Beauchamp, J. L.
TI Ion Funnel Augmented Mars Atmospheric Pressure Photoionization Mass
   Spectrometry for In Situ Detection of Organic Molecules
SO JOURNAL OF THE AMERICAN SOCIETY FOR MASS SPECTROMETRY
LA English
DT Article
DE Ion Funnel; Mars; Photoionization
ID CORONENE; CATIONS
AB Laser desorption is an attractive technique for in situ sampling of organics on Mars given its relative simplicity. We demonstrate that under simulated Martian conditions (similar to 2.5 Torr CO2) laser desorption of neutral species (e. g., polycyclic aromatic hydrocarbons), followed by ionization with a simple ultraviolet light source such as a discharge lamp, offers an effective means of sampling organics for detection and identification with a mass spectrometer. An electrodynamic ion funnel is employed to provide efficient ion collection in the ambient Martian environment. This experimental methodology enables in situ sampling of Martian organics with minimal complexity and maximum flexibility.
C1 [Johnson, Paul V.; Hodyss, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Beauchamp, J. L.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
RP Johnson, PV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Paul.V.Johnson@jpl.nasa.gov
RI Johnson, Paul/D-4001-2009
OI Johnson, Paul/0000-0002-0186-8456
FU National Aeronautics and Space Administration; JPL's internal Research
   and Technology Development program
FX This research was carried out at the Division of Chemistry and Chemical
   Engineering and the Mass Spectrometry Resource Center in the Beckman
   Institute at the California Institute of Technology and at the Jet
   Propulsion Laboratory (JPL), California Institute of Technology, under a
   contract with the National Aeronautics and Space Administration and
   funded through JPL's internal Research and Technology Development
   program. Copyright 2014. All rights reserved. Government sponsorship is
   acknowledged.
NR 18
TC 4
Z9 4
U1 4
U2 27
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1044-0305
EI 1879-1123
J9 J AM SOC MASS SPECTR
JI J. Am. Soc. Mass Spectrom.
PD NOV
PY 2014
VL 25
IS 11
BP 1832
EP 1840
DI 10.1007/s13361-014-0930-z
PG 9
WC Biochemical Research Methods; Chemistry, Analytical; Chemistry,
   Physical; Spectroscopy
SC Biochemistry & Molecular Biology; Chemistry; Spectroscopy
GA AR9NO
UT WOS:000343902100002
PM 24986759
ER

PT J
AU Madzunkov, SM
   Nikolic, D
AF Madzunkov, Stojan M.
   Nikolic, Dragan
TI Accurate Xe Isotope Measurement Using JPL Ion Trap
SO JOURNAL OF THE AMERICAN SOCIETY FOR MASS SPECTROMETRY
LA English
DT Article
DE Quadrupole ion trap; Isotopic abundances
ID MASS-SPECTROMETRY; NOBLE-GASES; METEORITES; FRACTIONATION; XENON; EARTH;
   STARDUST; EJECTION; TIME
AB We report an approach for the reproducible and accurate compositional analysis of different mixtures of Xe isotopes using miniature Jet Propulsion Laboratory Quadrupole Ion Trap (JPL-QIT). A major study objective was to validate the recent instrumental improvements to the long-term operational stability under different pressures, temperatures, and trapping conditions. We propose that the present device can be used in certification of trace amounts of isotopes in mixtures dominated by one or more isotopes. Measured isotopic compositions are verified against commercially available standards with accuracy better than 0.07%. To aid the analysis of experimental data, we developed a scalable replica fitting method and use peak areas as descriptors of relative isotopic abundances. This low-power and low-mass device is ideally suited for planetary explorations aimed to enhance quantitative analysis for major isotopes present in small amounts of atmospheric samples.
C1 [Madzunkov, Stojan M.; Nikolic, Dragan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Madzunkov, SM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM stojan.madzunkov@jpl.nasa.gov
RI Nikolic, Dragan/N-8346-2015
OI Nikolic, Dragan/0000-0002-3810-7984
FU National Aeronautics and Space Administration; JPL's Research and
   Technology Development Program; U.S. Government
FX The authors are indebted to Rembrandt T. Schaefer (JPL) for his
   continuous technical support and expertise in electronics. They
   acknowledge the dedication of Jurij Simcic (JPL) to the initial peak
   height analysis as well as the design of the electron gun. The samples
   were prepared by Evan L. Neidholdt (JPL). The authors thank Professor
   Kenneth A. Farley (California Institute of Technology) for valuable
   comments on the manuscript. They also benefited from discussions with
   Murray R. Darrach (JPL), who shared his insight and enthusiasm during
   the course of this work. The research was carried out at the Jet
   Propulsion Laboratory, California Institute of Technology, under a
   contract with the National Aeronautics and Space Administration. It was
   supported by the JPL's Research and Technology Development Program.
   Copyright 2014 California Institute of Technology; U.S. Government
   sponsorship is acknowledged.
NR 35
TC 2
Z9 2
U1 2
U2 11
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1044-0305
EI 1879-1123
J9 J AM SOC MASS SPECTR
JI J. Am. Soc. Mass Spectrom.
PD NOV
PY 2014
VL 25
IS 11
BP 1841
EP 1852
DI 10.1007/s13361-014-0980-2
PG 12
WC Biochemical Research Methods; Chemistry, Analytical; Chemistry,
   Physical; Spectroscopy
SC Biochemistry & Molecular Biology; Chemistry; Spectroscopy
GA AR9NO
UT WOS:000343902100003
PM 25216693
ER

PT J
AU Witasse, O
   Duxbury, T
   Chicarro, A
   Altobelli, N
   Andert, T
   Aronica, A
   Barabash, S
   Bertaux, JL
   Bibring, JP
   Cardesin-Moinelo, A
   Cichetti, A
   Companys, V
   Dehant, V
   Denis, M
   Formisano, V
   Futaana, Y
   Giuranna, M
   Gondet, B
   Heather, D
   Hoffmann, H
   Holmstrom, M
   Manaud, N
   Martin, P
   Matz, KD
   Montmessin, F
   Morley, T
   Mueller, M
   Neukum, G
   Oberst, J
   Orosei, R
   Patzold, M
   Picardi, G
   Pischel, R
   Plaut, JJ
   Reberac, A
   Voss, PP
   Roatsch, T
   Rosenblatt, P
   Remus, S
   Schmedemann, N
   Willner, K
   Zegers, T
AF Witasse, O.
   Duxbury, T.
   Chicarro, A.
   Altobelli, N.
   Andert, T.
   Aronica, A.
   Barabash, S.
   Bertaux, J. -L.
   Bibring, J. -P
   Cardesin-Moinelo, A.
   Cichetti, A.
   Companys, V.
   Dehant, V.
   Denis, M.
   Formisano, V.
   Futaana, Y.
   Giuranna, M.
   Gondet, B.
   Heather, D.
   Hoffmann, H.
   Holmstrom, M.
   Manaud, N.
   Martin, P.
   Matz, K. -D.
   Montmessin, F.
   Morley, T.
   Mueller, M.
   Neukum, G.
   Oberst, J.
   Orosei, R.
   Patzold, M.
   Picardi, G.
   Pischel, R.
   Plaut, J. J.
   Reberac, A.
   Pardo Voss, P.
   Roatsch, T.
   Rosenblatt, P.
   Remus, S.
   Schmedemann, N.
   Willner, K.
   Zegers, T.
TI Mars Express investigations of Phobos and Deimos
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Phobos; Deimos; Moons; Mars; Mars Express; Flyby
ID ASTROMETRIC OBSERVATIONS; MARTIAN SATELLITES; SRC; MISSION; GROOVES;
   ORBITS; CAMERA; ORIGIN; MOONS
AB The Mars Express mission was launched in June 2003 and was inserted into orbit around Mars in December 2003. Its main objective is to study the Mars' subsurface, surface, atmosphere and interaction with the solar wind. A secondary objective is to study the martian moons, in particular the largest one Phobos, thanks to a near polar and elliptical orbit which allows the spacecraft to perform close flybys about every five months. The Mars Express data not only consist of high-resolution 3D color images, but also astrometric images, spectra from 0.18 to 20 mu m, radar echoes, Doppler signals from gravity experiments, and ion data. A new view of the moons has emerged from this data set, favoring now the idea that they are not captured asteroids, but rather the result of a re-accretion following a major impact on Mars. This unique set of data is available in the ESA Planetary Science Archive (PSA) and mirror imaged in the NASA Planetary Data System (PDS). This paper presents an overview of the Mars Express Phobos flybys, the specificities of their operations and the scientific achievements. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Witasse, O.; Chicarro, A.] European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands.
   [Duxbury, T.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA.
   [Altobelli, N.; Cardesin-Moinelo, A.; Heather, D.; Manaud, N.; Martin, P.; Pardo Voss, P.; Remus, S.] European Space Agcy, ESAC, Villanueva De La Canada, Spain.
   [Andert, T.] Univ Bundeswehr Munchen, Fak Luft & Raumfahrttech, Inst Raumfahrttech, D-85577 Neubiberg, Germany.
   [Aronica, A.; Cichetti, A.; Formisano, V.; Giuranna, M.; Orosei, R.] INAF Ist Nazl AstroFis, IAPS Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy.
   [Barabash, S.; Futaana, Y.; Holmstrom, M.] Swedish Inst Space Phys, SE-98128 Kiruna, Sweden.
   [Bertaux, J. -L.; Montmessin, F.; Reberac, A.] CNRS UVSQ IPSL, LATMOS, F-78280 Guyancourt, France.
   [Bibring, J. -P; Gondet, B.] Inst Astrophys Spatiale, F-91405 Orsay, France.
   [Companys, V.; Denis, M.; Morley, T.; Mueller, M.] European Space Agcy, ESOC, D-64293 Darmstadt, Germany.
   [Dehant, V.; Rosenblatt, P.] Royal Observ Belgium, B-1180 Brussels, Belgium.
   [Hoffmann, H.; Matz, K. -D.; Oberst, J.; Roatsch, T.] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany.
   [Neukum, G.; Schmedemann, N.] Free Univ Berlin, Inst Geol Sci Planetary Sci & Remote Sensing, D-12249 Berlin, Germany.
   [Patzold, M.] Univ Cologne, Rhein Inst Umweltforsch, Abt Planetenforsch, D-50931 Cologne, Germany.
   [Picardi, G.] Univ 15 Sapienza, Dipartimento Ingn Informaz Elettron & Telecomunic, Rome, Italy.
   [Pischel, R.] European Space Agcy, Moscow Off, Moscow, Russia.
   [Plaut, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Willner, K.] TU Berlin, Berlin, Germany.
   [Zegers, T.] European Commiss, Brussels, Belgium.
RP Witasse, O (reprint author), European Space Agcy, Estec, Keplerlaan 1, NL-2200 AG Noordwijk, Netherlands.
EM Olivier.Witasse@esa.int
OI Aronica, Alessandro/0000-0003-3205-9472; GIURANNA,
   Marco/0000-0001-8967-9184; Futaana, Yoshifumi/0000-0002-7056-3517
FU DLR [50QM1004, 50QM1002]; NASA; Prodex
FX The Mars Express mission is an exemplary international collaboration in
   space exploration. The MaRS team thanks the MEX Flight Control Team, the
   operators at the ESA New Norcia ground station antenna and at the NASA
   Deep Space Network complexes, Tommy Thompson and Padma Varanasi, both at
   JPL, for their continuous support. The MaRS team is funded by DLR Grants
   50QM1004, 50QM1002, by NASA and by Prodex. The MARSIS team thank the
   Space agencies ASI, ESA and NASA for the support to the MARSIS mission.
   A special thought goes to our colleague and friend Ali Safaeinili who
   passed away in July 2009. He was one of the great pioneers in the
   observation of Phobos and one of the most active scientists of the
   MARSIS radar team. O. Witasse thanks B. Keaton for text improvement.
NR 45
TC 15
Z9 15
U1 1
U2 13
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 NOV 1
PY 2014
VL 102
SI SI
BP 18
EP 34
DI 10.1016/j.pss.2013.08.002
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8QD
UT WOS:000343838800004
ER

PT J
AU Jacobson, RA
   Lainey, V
AF Jacobson, R. A.
   Lainey, V.
TI Martian satellite orbits and ephemerides
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Phobos; Deimos; Mars; Planetary satellites; Orbits
ID DEIMOS ASTROMETRIC OBSERVATIONS; MARS EXPRESS; PHOBOS MISSION;
   GRAVITY-FIELD; MOTION; SPACECRAFT; ESAPHO; SRC; LIBRATION; MARINER-9
AB We discuss the general characteristics of the orbits of the Martian satellites, Phobos and Deimos. We provide a concise review of the various descriptions of the orbits by both analytical theories and direct numerical integrations of their equations of motion. After summarizing the observational data used to determine the orbits, we discuss the results of our latest orbits obtained from a least squares fit to the data. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Jacobson, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
   [Lainey, V.] UPMC, CNRS, UMR 8028, Observ Paris,Inst Mecan Celeste & Calcul Ephemeri, F-75814 Paris, France.
RP Jacobson, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM robert.jacobson@jpl.nasa.gov
NR 82
TC 4
Z9 4
U1 0
U2 5
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 NOV 1
PY 2014
VL 102
SI SI
BP 35
EP 44
DI 10.1016/j.pss.2013.06.003
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8QD
UT WOS:000343838800005
ER

PT J
AU Patzold, M
   Andert, T
   Jacobson, R
   Rosenblatt, P
   Dehant, V
AF Paetzold, Martin
   Andert, Tom
   Jacobson, Robert
   Rosenblatt, Pascal
   Dehant, Veronique
TI Phobos: Observed bulk properties
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Phobos; Mass; Density; Origin
ID ASTEROID 21 LUTETIA; MASS DETERMINATION; MARS EXPRESS; EPHEMERIS;
   TRACKING; DENSITY; GRAVITY; ORBITS; FLYBYS; FIELD
AB This work is a review of the mass determinations of the Mars moon Phobos by spacecraft close flybys, by solving for the Martian gravity field and by the analysis of secular orbit perturbations. The absolute value and accuracy is sensitive on the knowledge and accuracy of the Phobos ephemeris, of the spacecraft orbit, other perturbing forces acting on the spacecraft and the resolution of the Martian gravity field besides the measurement accuracy of the radio tracking data. The mass value and its error improved from spacecraft mission to mission or from the modern analysis of "old" tracking data but these solutions depend on the accuracy of the ephemeris at the time of observation. The mass value seems to settle within the range of GM(Ph)=(7.11 +/- 0.09) x 10(-4) km(3) s(-2) which covers almost all mass values from close flybys and "distant" encounters within its 3-sigma error (1.5%). Using the volume value determined from MEX HRSC imaging, the bulk density is (1873 +/- 31) kg m(-3) (3-sigma error or 1.7%), a low value which suggests that Phobos is either highly porous, is composed partially of light material or both. The determination of the gravity coefficients C-20 and C-22 from the Mars Express 2010 close flyby does not allow to draw conclusion on the internal structure. The large errors do not distinguish whether Phobos is homogeneous or not. In view of theories of the Phobos' origin, one possibility is that Phobos is not a captured asteroid but accreted from a debris disk in Mars orbit as a second generation solar system object. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Paetzold, Martin] Univ Cologne, Rhein Inst Umweltforsch, Abt Planetenforsch, D-50931 Cologne, Germany.
   [Andert, Tom] Univ Bundeswehr Munchen, Inst Raumfahrttech & Weltraumnutzung, Neubiberg, Germany.
   [Jacobson, Robert] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Rosenblatt, Pascal; Dehant, Veronique] Royal Observ Belgium, Brussels, Belgium.
RP Patzold, M (reprint author), Univ Cologne, Rhein Inst Umweltforsch, Abt Planetenforsch, D-50931 Cologne, Germany.
EM mpaetzol@uni-koeln.de
FU International Space Science Institute (ISSI) in Bern, Switzerland;
   Deutsches Zentrum fur Luft- und Raumfahrt, Bonn-Oberkassel [50QM1004,
   50QM1005]; Prodex; NASA
FX The authors thank the International Space Science Institute (ISSI) in
   Bern, Switzerland, for the support and Jurgen Oberst and Maria Wahlisch
   for the organization of the Phobos study. Thanks to the Mars Express
   project members at ESTEC, ESOC, ESAC, the ESTRACK New Norcia ground
   station and the Deep Space Network for the continuous support of the
   MaRS experiment. MP and TA are supported by the Deutsches Zentrum fur
   Luft- und Raumfahrt, Bonn-Oberkassel, under grants 50QM1004 and
   50QM1005; PR and VD are supported by Prodex and RAJ is supported by
   NASA.
NR 38
TC 7
Z9 7
U1 1
U2 5
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 NOV 1
PY 2014
VL 102
SI SI
BP 86
EP 94
DI 10.1016/j.pss.2014.01.004
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8QD
UT WOS:000343838800010
ER

PT J
AU Zakharov, A
   Horanyi, M
   Lee, P
   Witasse, O
   Cipriani, F
AF Zakharov, Alexander
   Horanyi, Mihaly
   Lee, Pascal
   Witasse, Olivier
   Cipriani, Fabrice
TI Dust at the Martian moons and in the circummartian space
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Dust; Martian moons; Plasma; Dust tori; Particle dynamic
ID SOLAR-WIND INTERACTION; PHOBOS EVENTS; MARS; DEIMOS; TORUS; SIGNATURES;
   SEARCH; BELTS; RINGS; SATELLITE
AB The paper provides the current understanding of the dust particle dynamics near the surface and in the circummatrian space of the Martian moons based on existing models developed for airless and non-magnetized bodies. In particular we discuss the response of the regolith of the Martian moons to exposure to radiation, the dynamics of charged dust on their surfaces, their plasma environments, the models and indirect observations of their putative dust tori. It is concluded that there is a good theoretical understanding of the behavior of the dynamics of dust particles near the moons Phobos and Deimos. Current models predict dust rings near orbits of the Martian moons based on detailed estimates for the sources and sinks of the dust particles as well as their lifetimes. However, there is no compelling observational evidence for the predicted dust torus around Phobos or Deimos orbits, and there are no observations yet of dust dynamics near their surfaces. Naturally, in order to detect the motion of dust near the surfaces of these moons, and their dust tori we need measurements using a complementary set of sensitive instruments, including impart dust detectors, electric field sensors, and optical cameras in future missions to Mars and its moons. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Zakharov, Alexander] Space Res Inst, Moscow 117997, Russia.
   [Horanyi, Mihaly] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
   [Lee, Pascal] NASA, Ames Res Ctr, Mars Inst, Washington, DC USA.
   [Lee, Pascal] NASA, Ames Res Ctr, SETI Inst, Washington, DC USA.
   [Witasse, Olivier; Cipriani, Fabrice] Estec, ESA, Noordwijk, Netherlands.
RP Zakharov, A (reprint author), Space Res Inst, Profsojuznaja 84-32, Moscow 117997, Russia.
EM zakharov@iki.rssi.ru
OI Horanyi, Mihaly/0000-0002-5920-9226
FU International Space Science Institute; Program 22 of the Presidium of
   the Russian academy of sciences
FX The work was supported by International Space Science Institute and the
   Program 22 of the Presidium of the Russian academy of sciences. We are
   grateful to J. Oberst for inspiration of this paper and E. Dubinin for
   helpful remarks.
NR 47
TC 5
Z9 5
U1 1
U2 7
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 NOV 1
PY 2014
VL 102
SI SI
BP 171
EP 175
DI 10.1016/j.pss.2013.12.011
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR8QD
UT WOS:000343838800016
ER

PT J
AU Alvin, MA
   Klotz, K
   McMordie, B
   Zhu, D
   Gleeson, B
   Warnes, B
AF Alvin, M. A.
   Klotz, K.
   McMordie, B.
   Zhu, D.
   Gleeson, B.
   Warnes, B.
TI Extreme Temperature Coatings for Future Gas Turbine Engines
SO JOURNAL OF ENGINEERING FOR GAS TURBINES AND POWER-TRANSACTIONS OF THE
   ASME
LA English
DT Article
ID THERMAL BARRIER COATINGS
AB The National Energy Technology Laboratory-Regional University Alliance (NETL-RUA) has been developing extreme temperature coating systems that consist of a diffusion barrier coating (DBC), a low-cost wet slurry bond coat, a commercial yttria stabilized zirconia (YSZ) thermal barrier coating (TBC), and an extreme temperature external coating that are deposited along the surface of nickel-based superalloys and single crystal metal substrates. Thermal cyclic testing of these multilayer coatings was conducted in steam-containing environments at temperatures ranging between 1100 and 1550 degrees C. This paper discusses the response of these materials during bench-scale testing, and their potential use in advanced H- and J-class land-based gas turbine engines.
C1 [Alvin, M. A.] US DOE Natl Energy, Technol Lab, Pittsburgh, PA 15236 USA.
   [Klotz, K.; McMordie, B.] Coatings For Ind, Souderton, PA 18964 USA.
   [Zhu, D.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
   [Gleeson, B.] Univ Pittsburgh, Pittsburgh, PA 15261 USA.
   [Warnes, B.] Corrosion Control Consultants Inc, Beaver, PA 15009 USA.
RP Alvin, MA (reprint author), US DOE Natl Energy, Technol Lab, Pittsburgh, PA 15236 USA.
EM maryanne.alvin@netl.doe.gov
FU NETL [DE-FE-0004000.3.622.243.002]
FX We acknowledge Mr. Richard Dennis, DOE NETL Turbine Technology Manager,
   and Dr. Patcharin Burke for their technical support. Efforts were
   performed under NETL Contract DE-FE-0004000.3.622.243.002.
NR 11
TC 3
Z9 3
U1 2
U2 28
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0742-4795
EI 1528-8919
J9 J ENG GAS TURB POWER
JI J. Eng. Gas. Turbines Power-Trans. ASME
PD NOV
PY 2014
VL 136
IS 11
AR 112102
DI 10.1115/1.4027186
PG 8
WC Engineering, Mechanical
SC Engineering
GA AR5ZI
UT WOS:000343661200011
ER

PT J
AU Petropoulou, M
   Dimitrakoudis, S
   Mastichiadis, A
   Giannios, D
AF Petropoulou, M.
   Dimitrakoudis, S.
   Mastichiadis, A.
   Giannios, D.
TI Hadronic supercriticality as a trigger for gamma-ray burst emission
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE astroparticle physics; instabilities; radiation mechanisms: non-thermal;
   gamma-ray burst: general
ID ENERGY COSMIC-RAYS; ACTIVE GALACTIC NUCLEI; SELF-COMPTON EMISSION;
   PROMPT EMISSION; PAIR PRODUCTION; COMPACT SOURCES;
   SYNCHROTRON-RADIATION; PARTICLE-ACCELERATION; TEMPORAL SIGNATURES;
   SPECTRAL COMPONENT
AB We explore a one-zone hadronic model that may be able to reproduce gamma-ray burst (GRB) prompt emission with a minimum of free parameters. Assuming only that GRBs are efficient high-energy proton accelerators and without the presence of an ab initio photon field, we investigate the conditions under which the system becomes supercritical, i.e. there is a fast, non-linear transfer of energy from protons to secondary particles initiated by the spontaneous quenching of proton-produced gamma-rays. We first show analytically that the transition to supercriticality occurs whenever the proton injection compactness exceeds a critical value, which favours high proton injection luminosities and a wide range of bulk Lorentz factors. The properties of supercriticality are then studied with a time-dependent numerical code that solves concurrently the coupled equations of proton, photon, electron, neutron and neutrino distributions. For conditions that drive the system deep into the supercriticality, we find that the photon spectra obtain a Band-like shape due to Comptonization by cooled pairs and that the energy transfer efficiency from protons to gamma-rays and neutrinos is high reaching similar to 0.3. Although some questions concerning its full adaptability to the GRB prompt emission remain open, supercriticality is found to be a promising process in that regard.
C1 [Petropoulou, M.; Giannios, D.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
   [Dimitrakoudis, S.] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, Penteli 15236, Greece.
   [Mastichiadis, A.] Univ Athens, Dept Phys, GR-15783 Zografos, Greece.
RP Petropoulou, M (reprint author), NASA, Washington, DC 20456 USA.
EM maroulaaki@gmail.com
RI Dimitrakoudis, Stavros/C-8591-2014; Petropoulou, Maria/L-6790-2016
OI Dimitrakoudis, Stavros/0000-0002-3368-3739; Petropoulou,
   Maria/0000-0001-6640-0179
FU NASA through Einstein Postdoctoral Fellowship grant - Chandra X-ray
   Center [PF 140113]; NASA [NAS8-03060]; Fermi six cycle grant [61122]
FX Support for this work was provided by NASA through Einstein Postdoctoral
   Fellowship grant number PF 140113 awarded by the Chandra X-ray Center,
   which is operated by the Smithsonian Astrophysical Observatory for NASA
   under contract NAS8-03060. DG acknowledges support from the Fermi six
   cycle grant number 61122.
NR 106
TC 1
Z9 1
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 NOV 1
PY 2014
VL 444
IS 3
BP 2186
EP 2199
DI 10.1093/mnras/stu1362
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR2FS
UT WOS:000343399600018
ER

PT J
AU Panopoulou, GV
   Tassis, K
   Goldsmith, PF
   Heyer, MH
AF Panopoulou, G. V.
   Tassis, K.
   Goldsmith, P. F.
   Heyer, M. H.
TI (CO)-C-13 filaments in the Taurus molecular cloud
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: formation; ISM: clouds; ISM: individual objects: Taurus; ISM:
   molecules; ISM: structure; radio lines: ISM
ID GOULD BELT SURVEY; INITIAL CONDITIONS; PRESTELLAR CORES; STAR-FORMATION;
   HERSCHEL; KINEMATICS; ACCRETION; COMPLEX; REGION; L1506
AB We have carried out a search for filamentary structures in the Taurus molecular cloud using (CO)-C-13 line emission data from the Five Colleges Radio Astronomy Observatory survey of similar to 100 deg(2). We have used the topological analysis tool, Discrete Persistent Structures Extractor (DISPERSE), and post-processed its results to include a more strict definition of filaments that requires an aspect ratio of at least 3:1 and cross-section intensity profiles peaked on the spine of the filament. In the velocity-integrated intensity map only 10 of the hundreds of filamentary structures identified by DISPERSE comply with our criteria. Unlike Herschel analyses, which find a characteristic width for filaments of similar to 0.1 pc, we find a much broader distribution of profile widths in our structures, with a peak at 0.4 pc. Furthermore, even if the identified filaments are cylindrical objects, their complicated velocity structure and velocity dispersions imply that they are probably gravitationally unbound. Analysis of velocity channel maps reveals the existence of hundreds of 'velocity-coherent' filaments. The distribution of their widths is peaked at lower values (0.2 pc) while the fluctuation of their peak intensities is indicative of stochastic origin. These filaments are suppressed in the integrated intensity map due to the blending of diffuse emission from different velocities. Conversely, integration over velocities can cause filamentary structures to appear. Such apparent filaments can also be traced, using the same methodology, in simple simulated maps consisting of randomly placed cores. They have profile shapes similar to observed filaments and contain most of the simulated cores.
C1 [Panopoulou, G. V.; Tassis, K.] Univ Crete, Dept Phys, Iraklion 71003, Greece.
   [Panopoulou, G. V.; Tassis, K.] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Crete, Greece.
   [Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Heyer, M. H.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
RP Panopoulou, GV (reprint author), Univ Crete, Dept Phys, POB 2208, Iraklion 71003, Greece.
EM panopg@physics.uoc.gr
RI Tassis, Konstantinos/C-3155-2011; Goldsmith, Paul/H-3159-2016
FU FP7 through Marie Curie Career Integration Grant [PCIG- GA-2011-293531
   FOnset]; EU FP7 Grant [PIRSES-GA-2012-31578 EuroCal]; RoboPol project;
   European Social Fund (ESF); Greek National Resources
FX KT acknowledges support by FP7 through Marie Curie Career Integration
   Grant PCIG- GA-2011-293531 FOnset.; KT and GVP would like to acknowledge
   partial support from the EU FP7 Grant PIRSES-GA-2012-31578 EuroCal.; GVP
   acknowledges support by the RoboPol project, which is implemented under
   the ARISTEIA Action of the OPERATIONAL PROGRAMME EDUCATION AND LIFELONG
   LEARNING and is co-funded by the European Social Fund (ESF) and Greek
   National Resources.
NR 40
TC 11
Z9 11
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV 1
PY 2014
VL 444
IS 3
BP 2507
EP 2524
DI 10.1093/mnras/stu1601
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR2FS
UT WOS:000343399600043
ER

PT J
AU Wang, L
   Viero, M
   Clarke, C
   Bock, J
   Buat, V
   Conley, A
   Farrah, D
   Guo, K
   Heinis, S
   Magdis, G
   Marchetti, L
   Marsden, G
   Norberg, P
   Oliver, SJ
   Page, MJ
   Roehlly, Y
   Roseboom, IG
   Schulz, B
   Smith, AJ
   Vaccari, M
   Zemcov, M
AF Wang, L.
   Viero, M.
   Clarke, C.
   Bock, J.
   Buat, V.
   Conley, A.
   Farrah, D.
   Guo, K.
   Heinis, S.
   Magdis, G.
   Marchetti, L.
   Marsden, G.
   Norberg, P.
   Oliver, S. J.
   Page, M. J.
   Roehlly, Y.
   Roseboom, I. G.
   Schulz, B.
   Smith, A. J.
   Vaccari, M.
   Zemcov, M.
TI HerMES: point source catalogues from Herschel-SPIRE observations II
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: statistical; techniques: photometric; catalogues; surveys;
   infrared: galaxies; submillimetre: galaxies
ID GALAXY NUMBER COUNTS; SOURCE EXTRACTION; MU-M; INSTRUMENT; SYSTEM;
   IMAGES; LASSO
AB The Herschel Multi-tiered Extragalactic Survey (HerMES) is the largest Guaranteed Time Key Programme on the Herschel Space Observatory. With a wedding cake survey strategy, it consists of nested fields with varying depth and area totalling similar to 380 deg(2). In this paper, we present deep point source catalogues extracted from Herschel-Spectral and Photometric Imaging Receiver (SPIRE) observations of all HerMES fields, except for the later addition of the 270 deg(2) HerMES Large-Mode Survey (HeLMS) field. These catalogues constitute the second Data Release (DR2) made in 2013 October. A sub-set of these catalogues, which consists of bright sources extracted from Herschel-SPIRE observations completed by 2010 May 1 (covering similar to 74 deg(2)) were released earlier in the first extensive data release in 2012 March. Two different methods are used to generate the point source catalogues, the SUSSEXTRACTOR point source extractor used in two earlier data releases (EDR and EDR2) and a new source detection and photometry method. The latter combines an iterative source detection algorithm, STARFINDER, and a De-blended SPIRE Photometry algorithm. We use end-to-end Herschel-SPIRE simulations with realistic number counts and clustering properties to characterize basic properties of the point source catalogues, such as the completeness, reliability, photometric and positional accuracy. Over 500 000 catalogue entries in HerMES fields (except HeLMS) are released to the public through the HeDAM (Herschel Database in Marseille) website (http://hedam.lam.fr/HerMES).
C1 [Wang, L.; Clarke, C.; Farrah, D.; Guo, K.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
   [Wang, L.; Norberg, P.] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England.
   [Viero, M.; Bock, J.; Schulz, B.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA.
   [Bock, J.; Zemcov, M.] Jet Prop Lab, Pasadena, CA 91109 USA.
   [Buat, V.; Heinis, S.; Roehlly, Y.] Univ Aix Marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France.
   [Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
   [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
   [Guo, K.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China.
   [Magdis, G.; Vaccari, M.] Univ Oxford, Oxford OX1 3RH, England.
   [Marchetti, L.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
   [Marchetti, L.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
   [Marsden, 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.
   [Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
   [Schulz, B.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
   [Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa.
RP Wang, L (reprint author), Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
EM lingyu.wang25@gmail.com
RI Magdis, Georgios/C-7295-2014; Vaccari, Mattia/R-3431-2016; 
OI Magdis, Georgios/0000-0002-4872-2294; Vaccari,
   Mattia/0000-0002-6748-0577; Marchetti, Lucia/0000-0003-3948-7621
FU UK's Science and Technology Facilities Council [ST/F002858/1]; ERC StG
   grant [DEGAS-259586]; CSA (Canada); NAOC (China); CEA (France); CNES
   (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC
   (UK); NASA (USA)
FX LW is supported by UK's Science and Technology Facilities Council grant
   ST/F002858/1 and an ERC StG grant (DEGAS-259586). The data presented in
   this paper will be released through the HeDaM (hedam.lam.fr/HerMES).
   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); 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).
NR 30
TC 25
Z9 25
U1 0
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 NOV 1
PY 2014
VL 444
IS 3
BP 2870
EP 2883
DI 10.1093/mnras/stu1569
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR2FS
UT WOS:000343399600066
ER

PT J
AU Barnell, TJ
   Rauscher, MD
   Doudican, BM
   Sutter, JK
AF Barnell, T. J.
   Rauscher, M. D.
   Doudican, B. M.
   Sutter, J. K.
TI No-Oven, No-Autoclave (NONA) Processing for NASA Composite Structures
SO SAMPE JOURNAL
LA English
DT Article
AB Cornerstone Research Group's (CRG) no-oven, no-autoclave (NOM) composite processing enables the fabrication of high-performance composite parts without the limitations imposed by autoclaves and ovens. We are actively expanding the NONA technology toolbox to enable fabrication of large, single-piece composite structures and to provide a low-cost manufacturing option for high-performance composite tooling We have worked with NASA to significantly advance the technology readiness level (TRL) of NONA. Recognizing the challenges faced in the fabrication and use of composite tooling we have examined NONA performance in maintaining vacuum integrity through cyclic thermal and mechanical loading, dimensional accuracy of both tool and finished parts, coefficient of thermal expansion (CTE) compatibility, quality surface finish, and infusion process compatibility. We have demonstrated these capabilities at various scales, including the fabrication of a NONA honey-comb sandwich structure with a 127 cm x 66 cm core and a 117 cm x 107 cm curved NONA composite tool for fabrication of test panels relevant to NASA's Space Launch System (SLS). We have nearly completed a comprehensive mechanical characterization of NONA carbon composites for comparison to benchmark aerospace material systems.
C1 [Barnell, T. J.; Rauscher, M. D.; Doudican, B. M.] Cornerstone Res Grp Inc, Dayton, OH 45440 USA.
   [Sutter, J. K.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Barnell, TJ (reprint author), Cornerstone Res Grp Inc, Dayton, OH 45440 USA.
EM barnelltj@crgrp.com
NR 5
TC 0
Z9 0
U1 1
U2 9
PU SAMPE PUBLISHERS
PI COVINA
PA 1161 PARKVIEW DRIVE, COVINA, CA 91722 USA
SN 0091-1062
J9 SAMPE J
JI Sampe J.
PD NOV-DEC
PY 2014
VL 50
IS 6
BP 46
EP 55
PG 10
WC Engineering, Multidisciplinary; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA AR6KQ
UT WOS:000343692900006
ER

PT J
AU Singh, HB
AF Singh, Hanwant B.
TI Editorial for Peter Brimblecombe Virtual Special Issue (VSI)
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Editorial Material
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Singh, HB (reprint author), NASA, Ames Res Ctr, Mail Stop 245-5, Moffett Field, CA 94035 USA.
EM Hanwant.B.Singh@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD NOV
PY 2014
VL 97
SI SI
BP A4
EP A5
DI 10.1016/j.atmosenv.2014.06.059
PG 2
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AR1HQ
UT WOS:000343336700002
ER

PT J
AU Moore, JG
   Ruple, A
   Ballenger-Bass, K
   Bell, S
   Pennington, PL
   Scott, GI
AF Moore, J. Gooch
   Ruple, A.
   Ballenger-Bass, K.
   Bell, S.
   Pennington, P. L.
   Scott, G. I.
TI Snapshot of Vibrio parahaemolyticus densities in open and closed
   shellfish beds in Coastal South Carolina and Mississippi
SO ENVIRONMENTAL MONITORING AND ASSESSMENT
LA English
DT Article
DE Oysters; Surface water; Vibrio parahaemolyticus; Open and closed
   shellfish areas; Atlantic coast; Gulf coast
ID GULF-OF-MEXICO; UNITED-STATES; ESTUARINE ENVIRONMENT; MOLLUSCAN
   SHELLFISH; SHELLSTOCK OYSTERS; PREDICTIVE MODEL; CHESAPEAKE BAY; RAW
   OYSTERS; NEW-YORK; VULNIFICUS
AB Vibrio parahaemolyticus is a Gram negative, halophilic bacterium that is ubiquitous in warm, tropical waters throughout the world. It is a major cause of seafood-associated gastroenteritis and is generally associated with consumption of raw or undercooked seafood, especially oysters. This study presents a snapshot of total V. parahaemolyticus densities in surface waters and shellstock American oysters (Crassostrea virginica) from open and closed shellfish harvesting areas, as well as "more rural areas" on two different US coasts, the Atlantic and the Gulf. Sampling was conducted from 2001 to 2003 at five sites near Charleston/Georgetown, SC and at four locations in the Gulfport/Pascagoula, MS area. V. parahaemolyticus numbers were determined by a direct plating method using an alkaline-phosphatase-labeled DNA probe targeting the species-specific thermolabile hemolysin gene (tlh) that was used for identification of bacterial isolates. The greatest difference between the two coasts was salinity; mean salinity in SC surface waters was 32.9 ppt, whereas the mean salinity in MS waters was 19.2 ppt, indicating more freshwater input into MS shellfish harvesting areas during the study period. The mean V. parahaemolyticus numbers in oysters were almost identical between the two states (567.4 vs. 560.1 CFU/g). Bacterial numbers in the majority of surface water samples from both states were at or below the limit of detection (LOD = < 10 CFU/mL). The bacterial concentrations determined during this study predict a low public health risk from consumption of oysters in shellfish growing areas on either the Gulf or the Atlantic US coast.
C1 [Moore, J. Gooch; Ballenger-Bass, K.; Pennington, P. L.; Scott, G. I.] NOAA, NOS, NCCOS, Ctr Coastal Environm Hlth & Biomol Res CCEHBR Lab, Charleston, SC 29405 USA.
   [Ruple, A.; Bell, S.] Natl Marine Fisheries Serv, Off Sustainable Fisheries, NSIL, Pascagoula, MS USA.
RP Moore, JG (reprint author), NOAA, NOS, NCCOS, Ctr Coastal Environm Hlth & Biomol Res CCEHBR Lab, Charleston, SC 29405 USA.
EM janet.moore@noaa.gov
FU NOAA Aquatic Invasive Species Council
FX The National Oceanic and Atmospheric Administration (NOAA), National
   Ocean Service (NOS) does not approve, recommend, or endorse any
   proprietary product or material mentioned in this publication. Partial
   funding for this project was provided by a grant from the NOAA Aquatic
   Invasive Species Council (Dorn Carlson & Dean Wilkinson). We thank Ben
   Whaley and Harry Seel with South SCDHEC, AK Leight, Blaine West, and
   Rusty Day at the NOAA CCEHBR Lab for sample collection and transport to
   the Lab in Charleston, SC. We are grateful to James Daugomah at the NOAA
   CCEHBR Lab for creating GIS maps of sampling sites. We also thank the
   Mississippi Department of Marine Resources, Fisheries Personnel, who
   collected samples and transported them to the NMFS, NSIL Lab in
   Pascagoula, Mississippi.
NR 42
TC 2
Z9 2
U1 0
U2 12
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-6369
EI 1573-2959
J9 ENVIRON MONIT ASSESS
JI Environ. Monit. Assess.
PD NOV
PY 2014
VL 186
IS 11
BP 7949
EP 7960
DI 10.1007/s10661-014-3979-z
PG 12
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA AQ8CU
UT WOS:000343051400074
PM 25106119
ER

PT J
AU Kim, WS
   Diaz-Calderon, A
   Peters, SF
   Carsten, JL
   Leger, C
AF Kim, Won S.
   Diaz-Calderon, Antonio
   Peters, Stephen F.
   Carsten, Joseph L.
   Leger, Chris
TI Onboard Centralized Frame Tree Database for Intelligent Space Operations
   of the Mars Science Laboratory Rover
SO IEEE TRANSACTIONS ON CYBERNETICS
LA English
DT Article
DE Flight software; frame tree; hierarchical database; human-robot
   interaction; quaternion; spacecraft commands
ID EXPLORATION ROVERS; VISUAL ODOMETRY; EQUATIONS; TRACKING; ATTITUDE;
   FLIGHT
AB Planetary surface science operations performed by robotic space systems frequently require pointing cameras at various objects and moving a robotic arm end effector tool toward specific targets. Earlier NASA Mars Exploration Rovers did not have the ability to compute actual coordinates for given object coordinate frame names and had to be provided with explicit coordinates. Since it sometimes takes hours to more than a day to get final approval of certain calculated coordinates for command uplink via the Earth-based mission operations procedures, a highly desired enhancement for future rovers was to have the onboard automated capability to compute the coordinates for a given frame name. The Mars Science Laboratory (MSL) rover mission is the first to have a centralized coordinate transform database to maintain the knowledge of spatial relations. This onboard intelligence significantly simplifies communication and control between Earth-based human mission operators and the robotic rover on Mars by supporting higher level abstraction of commands using object and target names instead of coordinates. More specifically, the spatial relations of many object frames are represented hierarchically in a tree data structure, called the frame tree. Individual frame transforms are populated by their respective modules that have specific knowledge of the frames. Through this onboard centralized frame tree database, client modules can query transforms between any two frames and support spacecraft commands that use any frames maintained in the frame tree. Various operational examples in the MSL mission that have greatly benefitted from this onboard centralized frame tree database are presented.
C1 [Kim, Won S.; Peters, Stephen F.; Carsten, Joseph L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
   [Diaz-Calderon, Antonio] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21218 USA.
   [Leger, Chris] Google Inc, Mountain View, CA 94043 USA.
RP Kim, WS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM won.s.kim@jpl.nasa.gov; antonio.diaz-calderon@jhuapl.edu;
   stephen.f.peters@jpl.nasa.gov; joseph.l.carsten@jpl.nasa.gov;
   leger@google.com
NR 30
TC 1
Z9 1
U1 0
U2 8
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2168-2267
EI 2168-2275
J9 IEEE T CYBERNETICS
JI IEEE T. Cybern.
PD NOV
PY 2014
VL 44
IS 11
SI SI
BP 2109
EP 2121
DI 10.1109/TCYB.2014.2301442
PG 13
WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics
SC Computer Science
GA AR1CT
UT WOS:000343319700011
PM 25330473
ER

PT J
AU Landi, E
   Bhatia, AK
AF Landi, E.
   Bhatia, A. K.
TI Atomic data and spectral line intensities for Ca IX
SO ATOMIC DATA AND NUCLEAR DATA TABLES
LA English
DT Article
DE Atomic data; Collision excitation rates; Radiative decay rates;
   Spectroscopic diagnostics; Spectral codes; Spectroscopy
ID ELECTRON-IMPACT EXCITATION; MAGNESIUM-LIKE IONS; MG-LIKE IONS;
   OSCILLATOR-STRENGTHS; RATE COEFFICIENTS; ENERGY-LEVELS; ISOELECTRONIC
   SEQUENCE; FORBIDDEN TRANSITIONS; EXTENDED ANALYSIS; NI-XVII
AB Electron impact collision strengths, energy levels, oscillator strengths, and spontaneous radiative decay rates are calculated for Ca IX. We include in the calculations the 33 lowest configurations in the n = 3, 4, and 5 complexes, corresponding to 283 fine-structure levels in the 3l3l', 3l4l '', and 3l5l'" configurations, where l, l' = s, p, d, l '' = s, p, d, f and l'" = s, p, d, f, g. Collision strengths are calculated at five incident energies for all transitions: 5.8, 13.6, 24.2, 38.6, and 57.9 Ry above the threshold of each transition. An additional energy, very close to the transition threshold, has been added, whose value is between 0.0055 Ry and 0.23 Ry depending on the levels involved. Calculations have been carried out using the Flexible Atomic Code and the distorted wave approximation. Excitation rate coefficients are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. Using the excitation rate coefficients and the radiative transition rates calculated in the present work, statistical equilibrium equations for level populations are solved at electron densities covering the range of 10(8)-10(14) cm(-3) and at an electron temperature of log T-e (K) = 5.8, corresponding to the maximum abundance of Ca IX. Spectral line intensities are calculated, and their diagnostic relevance is discussed. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Landi, E.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
   [Bhatia, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Landi, E (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM elandi@umich.edu
FU NASA [NNX10AQ58G, NNX11AC20G]; NSF [AGS-1154443]
FX The work of E. Landi is supported by NASA grants NNX10AQ58G and
   NNX11AC20G, as well as NSF grant AGS-1154443. Calculations were carried
   out using the Discover computer of the NASA Center for Computation
   Science. We thank the anonymous referee for her/his suggestions that
   helped improve the manuscript.
NR 44
TC 1
Z9 1
U1 0
U2 5
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0092-640X
EI 1090-2090
J9 ATOM DATA NUCL DATA
JI Atom. Data Nucl. Data Tables
PD NOV
PY 2014
VL 100
IS 6
BP 1519
EP 1592
DI 10.1016/j.adt.2014.03.002
PG 74
WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear
SC Physics
GA AQ7AM
UT WOS:000342965000003
ER

PT J
AU Truhlik, V
   Triskova, L
   Benson, RF
   Bilitza, D
   Grebowsky, J
   Richards, PG
AF Truhlik, Vladimir
   Triskova, Ludmila
   Benson, Robert F.
   Bilitza, Dieter
   Grebowsky, Joseph
   Richards, Phil G.
TI Comparison of H+ and He+ plasmapause locations based on the resurrected
   and reevaluated OGO-5 ion composition data base
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Plasmasphere; Plasmapause; FLIP; Empirical model; OGO-5
ID SOLAR-CYCLE VARIATIONS; ELECTRON-DENSITY; SATELLITE MEASUREMENTS; OUTER
   IONOSPHERE; EMPIRICAL-MODEL; PLASMASPHERE; DYNAMICS; MAGNETOSPHERE;
   TEMPERATURE; PROFILES
AB Orbiting Geophysical Observatory 5 (OGO 5) magnetospheric ion-composition data (H+, He+ and O+) have been retrieved from old magnetic tapes archived at the National Space Science Data Center (NSSDC). The highly compressed binary format was converted into a user-friendly ASCII format and these data have been made available online. We have inspected the reliability and consistency of this data set. Comparisons with the IRI-2012 climatological model and the FLIP theoretical model revealed a shift of absolute and relative ion densities with time. Here we have developed a correction procedure for the individual H+, He+ and O+ ion density measurements. We investigated plasmapause locations based on the density gradients in H+, and He+. The correlation coefficient between these locations was determined to be similar to 0.886 with the typical difference in L about 0.1. The electron density a the He+ plasmapause location based on the corrected data for all cases was > 100 cm(-3). (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Truhlik, Vladimir; Triskova, Ludmila] Acad Sci Czech Republic, Inst Atmospher Phys, Prague, Czech Republic.
   [Benson, Robert F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA.
   [Bilitza, Dieter; Richards, Phil G.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA.
   [Bilitza, Dieter] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA.
   [Grebowsky, Joseph] NASA, Planetary Magnetospheres Lab, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Truhlik, V (reprint author), Acad Sci Czech Republic, Inst Atmospher Phys, Prague, Czech Republic.
EM vtr@ufa.cas.cz; ltr@ufa.cas.cz; robert.f.benson@nasa.gov;
   dbilitza@gmu.edu; Joseph.M.Grebowsky@nasa.gov; prichar1@gmu.edu
RI Truhlik, Vladimir/H-6971-2014; Triskova, Ludmila/H-6503-2014
OI Truhlik, Vladimir/0000-0002-6624-4388; 
FU Ministry of Education, Youth and Sports of the Czech Republic [LH11123];
   NASA from the University of Colorado [NNX11AD7OG]; NASA from the NASA
   Geospace Program [NNX09AU37G]
FX This study was supported by Grant LH11123 of the Ministry of Education,
   Youth and Sports of the Czech Republic, by NASA Grant NNX11AD7OG under a
   subcontract to George Mason University from the University of Colorado,
   and by NASA Grant NNX09AU37G under a subcontract to George Mason
   University from the NASA Geospace Program.
NR 43
TC 0
Z9 0
U1 0
U2 7
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 NOV
PY 2014
VL 119
BP 27
EP 34
DI 10.1016/j.jastp.2014.06.007
PG 8
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA AQ6AQ
UT WOS:000342890100003
ER

PT J
AU Ade, PAR
   Aghanim, N
   Armitage-Caplan, C
   Arnaud, M
   Ashdown, M
   Atrio-Barandela, F
   Aumont, J
   Baccigalupi, C
   Banday, AJ
   Barreiro, RB
   Bartlett, JG
   Battaner, E
   Benabed, K
   Benoit, A
   Benoit-Levy, A
   Bernard, JP
   Bersanelli, M
   Bielewicz, P
   Bobin, J
   Bock, JJ
   Bonaldi, A
   Bond, JR
   Borrill, J
   Bouchet, FR
   Bridges, M
   Bucher, M
   Burigana, C
   Butler, RC
   Calabrese, E
   Cappellini, B
   Cardoso, JF
   Catalano, A
   Challinor, A
   Chamballu, A
   Chary, RR
   Chen, X
   Chiang, HC
   Chiang, LY
   Christensen, PR
   Church, S
   Clements, DL
   Colombi, S
   Colombo, LPL
   Couchot, F
   Coulais, A
   Crill, BP
   Curto, A
   Cuttaia, F
   Danese, L
   Davies, RD
   Davis, RJ
   de Bernardis, P
   de Rosa, A
   de Zotti, G
   Delabrouille, J
   Delouis, JM
   Desert, FX
   Dickinson, C
   Diego, JM
   Dolag, K
   Dole, H
   Donzelli, S
   Dore, O
   Douspis, M
   Dunkley, J
   Dupac, X
   Efstathiou, G
   Elsner, F
   Ensslin, TA
   Eriksen, HK
   Finelli, F
   Forni, O
   Frailis, M
   Fraisse, AA
   Franceschi, E
   Gaier, TC
   Galeotta, S
   Galli, S
   Ganga, K
   Giard, M
   Giardino, G
   Giraud-Heraud, Y
   Gjerlow, E
   Gonzalez-Nuevo, J
   Gorski, KM
   Gratton, S
   Gregorio, A
   Gruppuso, A
   Gudmundsson, JE
   Haissinski, J
   Hamann, J
   Hansen, FK
   Hanson, D
   Harrison, D
   Henrot-Versille, S
   Hernandez-Monteagudo, C
   Herranz, D
   Hildebrandt, SR
   Hivon, E
   Hobson, M
   Holmes, WA
   Hornstrup, A
   Hou, Z
   Hovest, W
   Huffenberger, KM
   Jaffe, AH
   Jaffe, TR
   Jewell, J
   Jones, WC
   Juvela, M
   Keihanen, E
   Keskitalo, R
   Kisner, TS
   Kneissl, R
   Knoche, J
   Knox, L
   Kunz, M
   Kurki-Suonio, H
   Lagache, G
   Lahteenmaki, A
   Lamarre, JM
   Lasenby, A
   Lattanzi, M
   Laureijs, RJ
   Lawrence, CR
   Leach, S
   Leahy, JP
   Leonardi, R
   Leon-Tavares, J
   Lesgourgues, J
   Lewis, A
   Liguori, M
   Lilje, PB
   Linden-Vornle, M
   Lopez-Caniego, M
   Lubin, PM
   Macias-Perez, JF
   Maffei, B
   Maino, D
   Mandolesi, N
   Maris, M
   Marshall, DJ
   Martin, PG
   Martinez-Gonzalez, E
   Masi, S
   Massardi, M
   Matarrese, S
   Matthai, F
   Mazzotta, P
   Meinhold, PR
   Melchiorri, A
   Melin, JB
   Mendes, L
   Menegoni, E
   Mennella, A
   Migliaccio, M
   Millea, M
   Mitra, S
   Miville-Deschenes, MA
   Moneti, A
   Montier, L
   Morgante, G
   Mortlock, D
   Moss, A
   Munshi, D
   Murphy, JA
   Naselsky, P
   Nati, F
   Natoli, P
   Netterfield, CB
   Norgaard-Nielsen, HU
   Noviello, F
   Novikov, D
   Novikov, I
   O'Dwyer, IJ
   Osborne, S
   Oxborrow, CA
   Paci, F
   Pagano, L
   Pajot, F
   Paladini, R
   Paoletti, D
   Partridge, B
   Pasian, F
   Patanchon, G
   Pearson, D
   Pearson, TJ
   Peiris, HV
   Perdereau, O
   Perotto, L
   Perrotta, F
   Pettorino, V
   Piacentini, F
   Piat, M
   Pierpaoli, E
   Pietrobon, D
   Plaszczynski, S
   Platania, P
   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
   Ristorcelli, I
   Rocha, G
   Rosset, C
   Roudier, G
   Rowan-Robinson, M
   Rubino-Martin, JA
   Rusholme, B
   Sandri, M
   Santos, D
   Savelainen, M
   Savini, G
   Scott, D
   Seiffert, MD
   Shellard, EPS
   Spencer, LD
   Starck, JL
   Stolyarov, V
   Stompor, R
   Sudiwala, R
   Sunyaev, R
   Sureau, F
   Sutton, D
   Suur-Uski, AS
   Sygnet, JF
   Tauber, JA
   Tavagnacco, D
   Terenzi, L
   Toffolatti, L
   Tomasi, M
   Tristram, M
   Tucci, M
   Tuovinen, J
   Turler, M
   Umana, G
   Valenziano, L
   Valiviita, J
   Van Tent, B
   Vielva, P
   Villa, F
   Vittorio, N
   Wade, A
   Wandelt, BD
   Wehus, IK
   White, M
   White, SDM
   Wilkinson, A
   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.
   Baccigalupi, C.
   Banday, A. J.
   Barreiro, R. B.
   Bartlett, J. G.
   Battaner, E.
   Benabed, K.
   Benoit, A.
   Benoit-Levy, A.
   Bernard, J. -P.
   Bersanelli, M.
   Bielewicz, P.
   Bobin, J.
   Bock, J. J.
   Bonaldi, A.
   Bond, J. R.
   Borrill, J.
   Bouchet, F. R.
   Bridges, M.
   Bucher, M.
   Burigana, C.
   Butler, R. C.
   Calabrese, E.
   Cappellini, B.
   Cardoso, J. -F.
   Catalano, A.
   Challinor, A.
   Chamballu, A.
   Chary, R. -R.
   Chen, X.
   Chiang, H. C.
   Chiang, L. -Y
   Christensen, P. R.
   Church, S.
   Clements, D. L.
   Colombi, S.
   Colombo, L. P. L.
   Couchot, F.
   Coulais, A.
   Crill, B. P.
   Curto, A.
   Cuttaia, F.
   Danese, L.
   Davies, R. D.
   Davis, R. J.
   de Bernardis, P.
   de Rosa, A.
   de Zotti, G.
   Delabrouille, J.
   Delouis, J. -M.
   Desert, F. -X.
   Dickinson, C.
   Diego, J. M.
   Dolag, K.
   Dole, H.
   Donzelli, S.
   Dore, O.
   Douspis, M.
   Dunkley, J.
   Dupac, X.
   Efstathiou, G.
   Elsner, F.
   Ensslin, T. A.
   Eriksen, H. K.
   Finelli, F.
   Forni, O.
   Frailis, M.
   Fraisse, A. A.
   Franceschi, E.
   Gaier, T. C.
   Galeotta, S.
   Galli, S.
   Ganga, K.
   Giard, M.
   Giardino, G.
   Giraud-Heraud, Y.
   Gjerlow, E.
   Gonzalez-Nuevo, J.
   Gorski, K. M.
   Gratton, S.
   Gregorio, A.
   Gruppuso, A.
   Gudmundsson, J. E.
   Haissinski, J.
   Hamann, J.
   Hansen, F. K.
   Hanson, D.
   Harrison, D.
   Henrot-Versille, S.
   Hernandez-Monteagudo, C.
   Herranz, D.
   Hildebrandt, S. R.
   Hivon, E.
   Hobson, M.
   Holmes, W. A.
   Hornstrup, A.
   Hou, Z.
   Hovest, W.
   Huffenberger, K. M.
   Jaffe, A. H.
   Jaffe, T. R.
   Jewell, J.
   Jones, W. C.
   Juvela, M.
   Keihanen, E.
   Keskitalo, R.
   Kisner, T. S.
   Kneissl, R.
   Knoche, J.
   Knox, L.
   Kunz, M.
   Kurki-Suonio, H.
   Lagache, G.
   Lahteenmaki, A.
   Lamarre, J. -M.
   Lasenby, A.
   Lattanzi, M.
   Laureijs, R. J.
   Lawrence, C. R.
   Leach, S.
   Leahy, J. P.
   Leonardi, R.
   Leon-Tavares, J.
   Lesgourgues, J.
   Lewis, A.
   Liguori, M.
   Lilje, P. B.
   Linden-Vornle, M.
   Lopez-Caniego, M.
   Lubin, P. M.
   Macias-Perez, J. F.
   Maffei, B.
   Maino, D.
   Mandolesi, N.
   Maris, M.
   Marshall, D. J.
   Martin, P. G.
   Martinez-Gonzalez, E.
   Masi, S.
   Massardi, M.
   Matarrese, S.
   Matthai, F.
   Mazzotta, P.
   Meinhold, P. R.
   Melchiorri, A.
   Melin, J. -B.
   Mendes, L.
   Menegoni, E.
   Mennella, A.
   Migliaccio, M.
   Millea, M.
   Mitra, S.
   Miville-Deschenes, M. -A.
   Moneti, A.
   Montier, L.
   Morgante, G.
   Mortlock, D.
   Moss, A.
   Munshi, D.
   Murphy, J. A.
   Naselsky, P.
   Nati, F.
   Natoli, P.
   Netterfield, C. B.
   Norgaard-Nielsen, H. U.
   Noviello, F.
   Novikov, D.
   Novikov, I.
   O'Dwyer, I. J.
   Osborne, S.
   Oxborrow, C. A.
   Paci, F.
   Pagano, L.
   Pajot, F.
   Paladini, R.
   Paoletti, D.
   Partridge, B.
   Pasian, F.
   Patanchon, G.
   Pearson, D.
   Pearson, T. J.
   Peiris, H. V.
   Perdereau, O.
   Perotto, L.
   Perrotta, F.
   Pettorino, V.
   Piacentini, F.
   Piat, M.
   Pierpaoli, E.
   Pietrobon, D.
   Plaszczynski, S.
   Platania, P.
   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.
   Ristorcelli, I.
   Rocha, G.
   Rosset, C.
   Roudier, G.
   Rowan-Robinson, M.
   Rubino-Martin, J. A.
   Rusholme, B.
   Sandri, M.
   Santos, D.
   Savelainen, M.
   Savini, G.
   Scott, D.
   Seiffert, M. D.
   Shellard, E. P. S.
   Spencer, L. D.
   Starck, J. -L.
   Stolyarov, V.
   Stompor, R.
   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.
   Tristram, M.
   Tucci, M.
   Tuovinen, J.
   Tuerler, M.
   Umana, G.
   Valenziano, L.
   Valiviita, J.
   Van Tent, B.
   Vielva, P.
   Villa, F.
   Vittorio, N.
   Wade, A.
   Wandelt, B. D.
   Wehus, I. K.
   White, M.
   White, S. D. M.
   Wilkinson, A.
   Yvon, D.
   Zacchei, A.
   Zonca, A.
TI Planck 2013 results. XVI. Cosmological parameters
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE cosmic background radiation; cosmological parameters; early Universe;
   inflation; primordial nucleosynthesis
ID MICROWAVE-ANISOTROPY-PROBE; BARYON ACOUSTIC-OSCILLATIONS; SOUTH-POLE
   TELESCOPE; HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; BACKGROUND POWER
   SPECTRUM; SUPERNOVA LEGACY SURVEY; INFLATIONARY UNIVERSE SCENARIO;
   PRIMORDIAL MAGNETIC-FIELDS; FINE-STRUCTURE CONSTANT
AB This paper presents the first cosmological results based on Planck measurements of the cosmic microwave background (CMB) temperature and lensing-potential power spectra. We find that the Planck spectra at high multipoles (l greater than or similar to 40) are extremely well described by the standard spatially-flat six-parameter ACDM cosmology with a power-law spectrum of adiabatic scalar perturbations. Within the context of this cosmology, the Planck data determine the cosmological parameters to high precision: the angular size of the sound horizon at recombination, the physical densities of baryons and cold dark matter, and the scalar spectral index are estimated to be theta* = (1.04147 +/- 0.00062) x 10(-2), Omega(b)h(2) = 0.02205 +/- 0.00028, Omega(c)h(2) = 0.1199 +/- 0.0027, and n(s) = 0.9603 +/- 0.0073, respectively (note that in this abstract we quote 68% errors on measured parameters and 95% upper limits on other parameters). For this cosmology, we find a low value of the Hubble constant, H-0 = (67.3 +/- 1.2) km s(-1) Mpc(-1), and a high value of the matter density parameter, Omega(m) = 0.315 +/- 0.017. These values are in tension with recent direct measurements of H-0 and the magnitude-redshift relation for Type Ia supernovae, but are in excellent agreement with geometrical constraints from baryon acoustic oscillation (BAO) surveys. Including curvature, we find that the Universe is consistent with spatial flatness to percent level precision using Planck CMB data alone. We use high-resolution CMB data together with Planck to provide greater control on extragalactic foreground components in an investigation of extensions to the six-parameter ACDM model. We present selected results from a large grid of cosmological models, using a range of additional astrophysical data sets in addition to Planck and high-resolution CMB data. None of these models are favoured over the standard six-parameter ACDM cosmology. The deviation of the scalar spectral index from unity is insensitive to the addition of tensor modes and to changes in the matter content of the Universe. We find an upper limit of r(0.002) < 0.11 on the tensor-to-scalar ratio. There is no evidence for additional neutrino-like relativistic particles beyond the three families of neutrinos in the standard model. Using BAO and CMB data, we find N-eff = 3.30 +/- 0.27 for the effective number of relativistic degrees of freedom, and an upper limit of 0.23 eV for the sum of neutrino masses. Our results are in excellent agreement with big bang nucleosynthesis and the standard value of N-eff = 3.046. We find no evidence for dynamical dark energy; using BAO and CMB data, the dark energy equation of state parameter is constrained to be w = -1.13(-0.10)(+0.13). We also use the Planck data to set limits on a possible variation of the fine-structure constant, dark matter annihilation and primordial magnetic fields. Despite the success of the six-parameter ACDM model in describing the Planck data at high multipoles, we note that this cosmology does not provide a good fit to the temperature power spectrum at low multipoles. The unusual shape of the spectrum in the multipole range 20 less than or similar to l less than or similar to 40 was seen previously in the WMAP data and is a real feature of the primordial CMB anisotropies.
   The poor fit to the spectrum at low multipoles is not of decisive significance, but is an "anomaly" in an otherwise self-consistent analysis of the Planck temperature data.
C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Sorbonne Paris Cite, APC, CNRS IN2P3,CEA Lrfu,Observ Paris, F-75205 Paris 13, France.
   [Lahteenmaki, A.; Leon-Tavares, J.; Poutanen, T.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland.
   [Kunz, M.] African Inst Math Sci, ZA-7950 Cape Town, South Africa.
   [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy.
   [Mandolesi, N.] Agenzia Spaziale Italiana, I-00198 Rome, Italy.
   [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
   [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa.
   [Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Santiago 0355, Chile.
   [Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
   [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France.
   [Bock, J. J.; Dore, O.; Hildebrandt, S. R.; Pearson, T. J.; Prezeau, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Pasadena, CA 91125 USA.
   [Challinor, A.; Shellard, E. P. S.] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Cambridge CB3 0WA, England.
   [Hernandez-Monteagudo, C.] CEFCA, Teruel 44001, Spain.
   [Borrill, J.; Keskitalo, R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
   [Rebolo, R.] CSIC, E-28006 Madrid, Spain.
   [Chamballu, A.; Melin, J. -B.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France.
   [Hornstrup, A.; Linden-Vornle, M.; Norgaard-Nielsen, H. U.; Oxborrow, C. A.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
   [Kunz, M.; Pettorino, V.; Tucci, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva, Switzerland.
   [Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain.
   [Toffolatti, L.] Univ Oviedo, Dept Fis, Oviedo 33007, Spain.
   [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
   [Rachen, J. P.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
   [Keskitalo, R.] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA.
   [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
   [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dana & David Dornsife Coll Letter, Dept Phys & Astron, Los Angeles, CA 90089 USA.
   [Benoit-Levy, A.; Peiris, H. V.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
   [Lewis, A.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
   [Huffenberger, K. M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA.
   [Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Poutanen, T.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland.
   [Chiang, H. C.; Fraisse, A. A.; Gudmundsson, J. E.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
   [White, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
   [Hou, Z.; Knox, L.; Liguori, M.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
   [Lubin, P. M.; Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
   [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA.
   [Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
   [Burigana, C.; Lattanzi, M.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy.
   [de Bernardis, P.; Masi, S.; Melchiorri, A.; Menegoni, E.; Nati, F.; Pagano, L.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
   [Bersanelli, M.; Maino, D.; Mennella, A.] Univ Milan, Dipartimento Fis, U-20133 Milan, Italy.
   [Gregorio, A.; Tavagnacco, D.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
   [Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
   [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark.
   [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
   [Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19001, Chile.
   [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid 28691, Spain.
   [Giardino, G.; Laureijs, R. J.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands.
   [Leon-Tavares, J.] Univ Turku, Finnish Ctr Astron, ESO FINCA, Piikkio 21500, Finland.
   [Partridge, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA.
   [Hovest, W.; Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland.
   [Umana, G.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy.
   [de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
   [Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
   [Frailis, M.; Galeotta, S.; Gregorio, A.; Maris, M.; Pasian, F.; Tavagnacco, D.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
   [Massardi, M.] Inst Radioastron, INAF, Bologna, Italy.
   [Burigana, C.; Butler, R. C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, I-40129 Bologna, Italy.
   [Bersanelli, M.; Cappellini, B.; Donzelli, S.; Maino, D.; Mennella, A.; Tomasi, M.] INAF IASF Milano, I-20133 Milan, Italy.
   [Finelli, F.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy.
   [Melchiorri, A.; Pagano, L.] Univ Roma La Sapienza, INFN, Sez Roma 1, I-00185 Rome, Italy.
   [Desert, F. -X.] Univ Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France.
   [Tuerler, M.] Univ Geneva, Data Ctr Astrophys, ISDC, CH-1290 Versoix, Switzerland.
   [Mitra, S.] IUCAA, Pune 411007, Maharashtra, India.
   [Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
   [Chary, R. -R.; Chen, X.; Paladini, R.; Pearson, T. J.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
   [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, F-38042 Grenoble, France.
   [Dole, H.] Inst Univ France, F-75005 Paris, France.
   [Aghanim, N.; Aumont, J.; Chamballu, A.; Dole, H.; Douspis, M.; Kunz, M.; Lagache, G.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Remazeilles, M.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, F-91405 Orsay, France.
   [Benabed, K.; Benoit, A.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Elsner, F.; Galli, S.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France.
   [Popa, L.] Inst Space Sci, Bucharest 077125, Romania.
   [Chiang, L. -Y; Ponthieu, N.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
   [Bridges, M.; Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
   [Eriksen, H. K.; Gjerlow, E.; Hansen, F. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
   [Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife 38200, Spain.
   [Barreiro, R. B.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain.
   [Platania, P.] CNR ENEA EURATOM Assoc, Ist Fis Plasma, I-20125 Milan, Italy.
   [Bartlett, J. G.; Bock, J. J.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gaier, T. C.; Gorski, K. M.; Hanson, D.; Holmes, W. A.; Jewell, J.; Lawrence, C. R.; Mitra, S.; O'Dwyer, I. J.; Pearson, D.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Roudier, G.; Seiffert, M. D.; Wade, A.; Wehus, I. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
   [Bonaldi, A.; Davies, R. D.; Davis, R. J.; Dickinson, C.; Leahy, J. P.; Maffei, B.; Noviello, F.; Remazeilles, M.; Wilkinson, A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
   [Ashdown, M.; Bridges, M.; Challinor, A.; Chamballu, A.; Gratton, S.; Harrison, D.; Lasenby, A.; Migliaccio, M.; Stolyarov, V.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
   [Couchot, F.; Haissinski, J.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, LAL, CNRS, IN2P3, F-91405 Orsay, France.
   [Catalano, A.; Coulais, A.; Lamarre, J. -M.; Roudier, G.] Observ Paris, CNRS, LERMA, F-75014 Paris, France.
   [Arnaud, M.; Bobin, J.; Marshall, D. J.; Pratt, G. W.; Starck, J. -L.; Sureau, F.] Univ Paris Diderot, CEA Saclay, Lab AIM, IRFU Serv Astrophys CEA DSM CNRS, F-91191 Gif Sur Yvette, France.
   [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France.
   [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France.
   [Catalano, A.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, Inst Natl Polytech Grenoble, CNRS IN2P3, F-38026 Grenoble, France.
   [Van Tent, B.] Univ Paris 11, Lab Phys Theor, F-91405 Orsay, France.
   [Van Tent, B.] CNRS, F-91405 Orsay, France.
   [Kisner, T. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
   [Dolag, K.; Ensslin, T. A.; Hernandez-Monteagudo, C.; Knoche, J.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.; Sunyaev, R.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
   [Hanson, D.] McGill Univ, Montreal, PQ H3A 2T8, Canada.
   [Tuovinen, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo 02044, Finland.
   [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland.
   [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
   [Crill, B. P.] CALTECH, Observ Cosmol, Pasadena, CA 91125 USA.
   [Savini, G.] UCL, Opt Sci Lab, London, England.
   [Lesgourgues, J.] Ecole Polytech Fed Lausanne, SB ITP LPPC, CH-1015 Lausanne, Switzerland.
   [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
   [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
   [Moss, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
   [Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia.
   [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Zelenchukskiy R, Russia.
   [Church, S.; Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
   [Armitage-Caplan, C.; Calabrese, E.; Dunkley, J.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England.
   [Hamann, J.; Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland.
   [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Delouis, J. -M.; Elsner, F.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR7095, F-75014 Paris, France.
   [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, IRAP, UPS OMP, F-31028 Toulouse 4, France.
   [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA.
   [Dolag, K.] Univ Munich, Univ Observ, D-81679 Munich, Germany.
   [Battaner, E.] Univ Granada, Dept Fis Teor & Cosmos, Fac Ciencias, E-18071 Granada, Spain.
   [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Efstathiou, G (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
EM gpe@ast.cam.ac.uk
RI Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo,
   Joaquin/I-3562-2014; Yvon, Dominique/D-2280-2015; Mazzotta,
   Pasquale/B-1225-2016; Colombo, Loris/J-2415-2016; Novikov,
   Igor/N-5098-2015; Nati, Federico/I-4469-2016; Novikov,
   Dmitry/P-1807-2015; Herranz, Diego/K-9143-2014; Vielva,
   Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; White,
   Martin/I-3880-2015; Atrio-Barandela, Fernando/A-7379-2017; Valiviita,
   Jussi/A-9058-2016; Kurki-Suonio, Hannu/B-8502-2016; Lahteenmaki,
   Anne/L-5987-2013; Lattanzi, Massimiliano/D-8120-2011; popa,
   lucia/B-4718-2012; Gruppuso, Alessandro/N-5592-2015; Tomasi,
   Maurizio/I-1234-2016; Pearson, Timothy/N-2376-2015; Stolyarov,
   Vladislav/C-5656-2017; Piacentini, Francesco/E-7234-2010; 
OI Galeotta, Samuele/0000-0002-3748-5115; Ricciardi,
   Sara/0000-0002-3807-4043; Juvela, Mika/0000-0002-5809-4834; Zacchei,
   Andrea/0000-0003-0396-1192; Scott, Douglas/0000-0002-6878-9840; Villa,
   Fabrizio/0000-0003-1798-861X; Hivon, Eric/0000-0003-1880-2733; TERENZI,
   LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach,
   William/0000-0001-8362-4094; Franceschi, Enrico/0000-0002-0585-6591;
   Mitra, Sanjit/0000-0002-0800-4626; Martinez-Gonzalez,
   Enrique/0000-0002-0179-8590; Gonzalez-Nuevo,
   Joaquin/0000-0003-1354-6822; Mazzotta, Pasquale/0000-0002-5411-1748;
   Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088;
   Herranz, Diego/0000-0003-4540-1417; Vielva,
   Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386;
   White, Martin/0000-0001-9912-5070; Atrio-Barandela,
   Fernando/0000-0002-2130-2513; Valiviita, Jussi/0000-0001-6225-3693;
   Kurki-Suonio, Hannu/0000-0002-4618-3063; Lattanzi,
   Massimiliano/0000-0003-1059-2532; Gruppuso,
   Alessandro/0000-0001-9272-5292; Tomasi, Maurizio/0000-0002-1448-6131;
   Pearson, Timothy/0000-0001-5213-6231; Stolyarov,
   Vladislav/0000-0001-8151-828X; Piacentini,
   Francesco/0000-0002-5444-9327; Lilje, Per/0000-0003-4324-7794; Paoletti,
   Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416;
   Pierpaoli, Elena/0000-0002-7957-8993
FU ESA; CNES; CNRS/INSU-IN2P3-INP (France)
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 and JA (Spain); Tekes, AoF and
   CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark);
   SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES
   (Portugal); and PRACE (EU). A description of the Planck Collaboration
   and a list of its members, including the technical or scientific
   activities in which they have been involved, can be found at
   http://www.sciops.esa.int/index.php?
   project=planck&page=Planck_Collaboration. We thank the referee for a
   comprehensive and helpful report. We also thank Jean-Philippe Uzan for
   his contributions to Sect. 6.8. We additionally acknowledge useful
   comments on the first version of this paper from a large number of
   scientists who have helped improve the clarity of the revised version.
   We mention specifically Jim Braatz, John Carlstrom, Alex Conley, Raphael
   Flauger, Liz Humphreys, Adam Riess, Beth Reid, Uros Seljak, David
   Spergel, Mark Sullivan, and Reynald Pain.
NR 359
TC 631
Z9 632
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 NOV
PY 2014
VL 571
AR A16
DI 10.1051/0004-6361/201321591
PG 66
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT9ZK
UT WOS:000345282600027
ER

PT J
AU Ade, PAR
   Aghanim, N
   Armitage-Caplan, C
   Arnaud, M
   Ashdown, M
   Atrio-Barandela, F
   Aumont, J
   Baccigalupi, C
   Banday, AJ
   Barreiro, RB
   Bartlett, JG
   Bartolo, N
   Battaner, E
   Benabed, K
   Benoit, A
   Benoit-Levy, A
   Bernard, JP
   Bersanelli, M
   Bielewicz, P
   Bobin, J
   Bock, JJ
   Bonaldi, A
   Bonavera, L
   Bond, JR
   Borrill, J
   Bouchet, FR
   Bridges, M
   Bucher, M
   Burigana, C
   Butler, RC
   Cardoso, JF
   Catalano, A
   Challinor, A
   Chamballu, A
   Chiang, HC
   Chiang, LY
   Christensen, PR
   Church, S
   Clements, DL
   Colombi, S
   Colombo, LPL
   Couchot, F
   Coulais, A
   Crill, BP
   Curto, A
   Cuttaia, F
   Danese, L
   Davies, RD
   Davis, RJ
   de Bernardis, P
   de Rosa, A
   de Zotti, G
   Delabrouille, J
   Delouis, JM
   Desert, FX
   Diego, JM
   Dole, H
   Donzelli, S
   Dore, O
   Douspis, M
   Ducout, A
   Dunkley, J
   Dupac, X
   Efstathiou, G
   Elsner, F
   Ensslin, TA
   Eriksen, HK
   Fergusson, J
   Finelli, F
   Forni, O
   Frailis, M
   Franceschi, E
   Galeotta, S
   Ganga, K
   Giard, M
   Giraud-Heraud, Y
   Gonzalez-Nuevo, J
   Gorski, KM
   Gratton, S
   Gregorio, A
   Gruppuso, A
   Hansen, FK
   Hanson, D
   Harrison, D
   Heavens, A
   Henrot-Versille, S
   Hernandez-Monteagudo, C
   Herranz, D
   Hildebrandt, SR
   Hivon, E
   Hobson, M
   Holmes, WA
   Hornstrup, A
   Hovest, W
   Huffenberger, KM
   Jaffe, AH
   Jaffe, TR
   Jones, WC
   Juvela, M
   Keihanen, E
   Keskitalo, R
   Kisner, TS
   Knoche, J
   Knox, L
   Kunz, M
   Kurki-Suonio, H
   Lacasa, F
   Lagache, G
   Lahteenmaki, A
   Lamarre, JM
   Lasenby, A
   Laureijs, RJ
   Lawrence, CR
   Leahy, JP
   Leonardi, R
   Lesgourgues, J
   Lewis, A
   Liguori, M
   Lilje, PB
   Linden-Vornle, M
   Lopez-Caniego, M
   Lubin, PM
   Macias-Perez, JF
   Maffei, B
   Maino, D
   Mandolesi, N
   Mangilli, A
   Marinucci, D
   Maris, M
   Marshall, DJ
   Martin, PG
   Martinez-Gonzalez, E
   Masi, S
   Massardi, M
   Matarrese, S
   Matthai, F
   Mazzotta, P
   Meinhold, PR
   Melchiorri, A
   Mendes, L
   Mennella, A
   Migliaccio, M
   Mitra, S
   Miville-Deschenes, MA
   Moneti, A
   Montier, L
   Morgante, G
   Mortlock, D
   Moss, A
   Munshi, D
   Murphy, JA
   Naselsky, P
   Natoli, P
   Netterfield, CB
   Norgaard-Nielsen, HU
   Noviello, F
   Novikov, D
   Novikov, I
   Osborne, S
   Oxborrowl, CA
   Paci, F
   Pagano, L
   Pajot, F
   Paoletti, D
   Pasian, F
   Patanchon, G
   Peiris, HV
   Perdereau, O
   Perotto, L
   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
   Racine, B
   Rebolo, R
   Reinecke, M
   Remazeilles, M
   Renault, C
   Renzi, A
   Ricciardi, S
   Riller, T
   Ristorcelli, I
   Rocha, G
   Rosset, C
   Roudier, G
   Rubino-Martin, JA
   Rusholme, B
   Sandri, M
   Santos, D
   Savini, G
   Scott, D
   Seiffert, MD
   Shellard, EPS
   Smith, K
   Spencer, LD
   Starck, JL
   Stolyarov, V
   Stompor, R
   Sudiwala, R
   Sunyaev, R
   Sureau, F
   Sutter, P
   Sutton, D
   Suur-Uski, AS
   Sygnet, JF
   Tauber, JA
   Tavagnacco, D
   Terenzi, L
   Toffolatti, L
   Tomasi, M
   Tristram, M
   Tucci, M
   Tuovinen, J
   Valenziano, L
   Valiviita, J
   Van Tent, B
   Varis, J
   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.
   Baccigalupi, C.
   Banday, A. J.
   Barreiro, R. B.
   Bartlett, J. G.
   Bartolo, N.
   Battaner, E.
   Benabed, K.
   Benoit, A.
   Benoit-Levy, A.
   Bernard, J. -P.
   Bersanelli, M.
   Bielewicz, P.
   Bobin, J.
   Bock, J. J.
   Bonaldi, A.
   Bonavera, L.
   Bond, J. R.
   Borrill, J.
   Bouchet, F. R.
   Bridges, M.
   Bucher, M.
   Burigana, C.
   Butler, R. C.
   Cardoso, J. -F.
   Catalano, A.
   Challinor, A.
   Chamballu, A.
   Chiang, H. C.
   Chiang, L. -Y
   Christensen, P. R.
   Church, S.
   Clements, D. L.
   Colombi, S.
   Colombo, L. P. L.
   Couchot, F.
   Coulais, A.
   Crill, B. P.
   Curto, A.
   Cuttaia, F.
   Danese, L.
   Davies, R. D.
   Davis, R. J.
   de Bernardis, P.
   de Rosa, A.
   de Zotti, G.
   Delabrouille, J.
   Delouis, J. -M.
   Desert, F. -X.
   Diego, J. M.
   Dole, H.
   Donzelli, S.
   Dore, O.
   Douspis, M.
   Ducout, A.
   Dunkley, J.
   Dupac, X.
   Efstathiou, G.
   Elsner, F.
   Ensslin, T. A.
   Eriksen, H. K.
   Fergusson, J.
   Finelli, F.
   Forni, O.
   Frailis, M.
   Franceschi, E.
   Galeotta, S.
   Ganga, K.
   Giard, M.
   Giraud-Heraud, Y.
   Gonzalez-Nuevo, J.
   Gorski, K. M.
   Gratton, S.
   Gregorio, A.
   Gruppuso, A.
   Hansen, F. K.
   Hanson, D.
   Harrison, D.
   Heavens, 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.
   Jaffe, A. H.
   Jaffe, T. R.
   Jones, W. C.
   Juvela, M.
   Keihanen, E.
   Keskitalo, R.
   Kisner, T. S.
   Knoche, J.
   Knox, L.
   Kunz, M.
   Kurki-Suonio, H.
   Lacasa, F.
   Lagache, G.
   Lahteenmaki, A.
   Lamarre, J. -M.
   Lasenby, A.
   Laureijs, R. J.
   Lawrence, C. R.
   Leahy, J. P.
   Leonardi, R.
   Lesgourgues, J.
   Lewis, A.
   Liguori, M.
   Lilje, P. B.
   Linden-Vornle, M.
   Lopez-Caniego, M.
   Lubin, P. M.
   Macias-Perez, J. F.
   Maffei, B.
   Maino, D.
   Mandolesi, N.
   Mangilli, A.
   Marinucci, D.
   Maris, M.
   Marshall, D. J.
   Martin, P. G.
   Martinez-Gonzalez, E.
   Masi, S.
   Massardi, M.
   Matarrese, S.
   Matthai, F.
   Mazzotta, P.
   Meinhold, P. R.
   Melchiorri, A.
   Mendes, L.
   Mennella, A.
   Migliaccio, M.
   Mitra, S.
   Miville-Deschenes, M. -A.
   Moneti, A.
   Montier, L.
   Morgante, G.
   Mortlock, D.
   Moss, A.
   Munshi, D.
   Murphy, J. A.
   Naselsky, P.
   Natoli, P.
   Netterfield, C. B.
   Norgaard-Nielsen, H. U.
   Noviello, F.
   Novikov, D.
   Novikov, I.
   Osborne, S.
   Oxborrowl, C. A.
   Paci, F.
   Pagano, L.
   Pajot, F.
   Paoletti, D.
   Pasian, F.
   Patanchon, G.
   Peiris, H. V.
   Perdereau, O.
   Perotto, L.
   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.
   Racine, B.
   Rebolo, R.
   Reinecke, M.
   Remazeilles, M.
   Renault, C.
   Renzi, A.
   Ricciardi, S.
   Riller, T.
   Ristorcelli, I.
   Rocha, G.
   Rosset, C.
   Roudier, G.
   Rubino-Martin, J. A.
   Rusholme, B.
   Sandri, M.
   Santos, D.
   Savini, G.
   Scott, D.
   Seiffert, M. D.
   Shellard, E. P. S.
   Smith, K.
   Spencer, L. D.
   Starck, J. -L.
   Stolyarov, V.
   Stompor, R.
   Sudiwala, R.
   Sunyaev, R.
   Sureau, F.
   Sutter, P.
   Sutton, D.
   Suur-Uski, A. -S.
   Sygnet, J. -F.
   Tauber, J. A.
   Tavagnacco, D.
   Terenzi, L.
   Toffolatti, L.
   Tomasi, M.
   Tristram, M.
   Tucci, M.
   Tuovinen, J.
   Valenziano, L.
   Valiviita, J.
   Van Tent, B.
   Varis, J.
   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. XXIV. Constraints on primordial non-Gaussianity
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE cosmic background radiation; cosmology: observations; cosmology: theory;
   early Universe; inflation; methods: data analysis
ID PROBE WMAP OBSERVATIONS; OBSERVATIONS COSMOLOGICAL INTERPRETATION;
   MICROWAVE BACKGROUND BISPECTRUM; NONLINEAR COUPLING PARAMETER; 3-POINT
   CORRELATION-FUNCTION; LARGE-SCALE STRUCTURE; MINKOWSKI FUNCTIONALS;
   COMPONENT SEPARATION; POINT SOURCES; POLARIZATION ANISOTROPIES
AB The Planck nominal mission cosmic microwave background (CMB) maps yield unprecedented constraints on primordial non-Gaussianity (NG). Using three optimal bispectrum estimators, separable template-fitting (KSW), binned, and modal, we obtain consistent values for the primordial local, equilateral, and orthogonal bispectrum amplitudes, quoting as our final result f(NL)(local) = 2.7 +/- 5.8, f(NL)(equil) = -42 +/- 75, and f(NL)(ortho) = 25 +/- 39 (68% CL statistical). Non-Gaussianity is detected in the data; using skew-C 'statistics we find a nonzero bispectrum from residual point sources, and the integrated-Sachs-Wolfe-lensing bispectrum at a level expected in the CDM scenario. The results are based on comprehensive crossvalidation of these estimators on Gaussian and non-Gaussian simulations, are stable across component separation techniques, pass an extensive suite of tests, and are confirmed by skew-C `, wavelet bispectrum and Minkowski functional estimators. Beyond estimates of individual shape amplitudes, we present model-independent, three-dimensional reconstructions of the Planck CMB bispectrum and thus derive constraints on early-Universe scenarios that generate primordial NG, including general single-field models of inflation, excited initial states (non-Bunch-Davies vacua), and directionally-dependent vector models. We provide an initial survey of scale-dependent feature and resonance models. These results bound both general single-field and multi-field model parameter ranges, such as the speed of sound, cs 0 : 02 (95% CL), in an e ff ective field theory parametrization, and the curvaton decay fraction rD 0 : 15 (95% CL). The Planck data significantly limit the viable parameter space of the ekpyrotic / cyclic scenarios. The amplitude of the four-point function in the local model NL < 2800 (95% CL). Taken together, these constraints represent the highest precision tests to date of physical mechanisms for the origin of cosmic structure.
C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Racine, B.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA Irfu,APC, F-75205 Paris 13, France.
   [Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland.
   [Kunz, M.] African Inst Math Sci, ZA-7945 Cape Town, South Africa.
   [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy.
   [Mandolesi, N.] Agenzia Spaziale Italiana, I-00998 Rome, Italy.
   [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
   [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa.
   [Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
   [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, TRAP, F-31028 Toulouse 4, France.
   [Bock, J. J.; Dore, O.; Hildebrandt, S. R.; Prezeau, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Pasadena, CA 91125 USA.
   [Challinor, A.; Fergusson, J.; Shellard, E. P. S.] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Cambridge CB3 0WA, England.
   [Hernandez-Monteagudo, C.] Ctr Estudios Fis Cosmos Aragon, Teruel 44001, Spain.
   [Borrill, J.; Keskitalo, R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
   [Rebolo, R.] CSIC, Madrid 2800, Spain.
   [Chamballu, A.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France.
   [Hornstrup, A.; Linden-Vornle, M.; Norgaard-Nielsen, H. U.; Oxborrowl, C. A.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
   [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland.
   [Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain.
   [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain.
   [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
   [Rachen, J. P.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
   [Keskitalo, R.] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA.
   [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
   [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA.
   [Benoit-Levy, A.; Peiris, H. V.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
   [Lewis, A.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
   [Huffenberger, K. M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA.
   [Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland.
   [Chiang, H. C.; Jones, W. C.; Smith, K.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
   [White, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
   [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
   [Lubin, P. M.; Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
   [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA.
   [Bartolo, N.; Liguori, M.; Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
   [Burigana, C.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy.
   [de Bernardis, P.; Masi, S.; Melchiorri, A.; Pagano, L.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
   [Bersanelli, M.; Maino, D.; Mennella, A.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy.
   [Gregorio, A.; Tavagnacco, D.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
   [Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartmento Fis, I-00133 Rome, Italy.
   [Marinucci, D.] Univ Roma Tor Vergata, Dipartimento Matemat, I-00133 Rome, Italy.
   [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark.
   [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
   [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid 28691, Spain.
   [Laureijs, R. J.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands.
   [Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland.
   [de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
   [Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
   [Frailis, M.; Galeotta, S.; Gregorio, A.; Maris, M.; Pasian, F.; Tavagnacco, D.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy.
   [Massardi, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
   [Burigana, C.; Butler, R. C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, I-40129 Bologna, Italy.
   [Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Tomasi, M.] INAF IASF Milano, I-20133 Milan, Italy.
   [Finelli, F.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy.
   [Melchiorri, A.; Pagano, L.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy.
   [Desert, F. -X.; Ponthieu, N.] Univ Grenoble 1, CNRS INSU, Inst Planetol & Astrophys Grenoble, UMR 5274, F-38041 Grenoble, France.
   [Mitra, S.] IUCAA, Pune 411007, Maharashtra, India.
   [Clements, D. L.; Heavens, A.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
   [Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
   [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, F-38042 Grenoble, France.
   [Dole, H.] Inst Univ France, F-75005 Paris, France.
   [Aghanim, N.; Aumont, J.; Chamballu, A.; Dole, H.; Douspis, M.; Kunz, M.; Lacasa, F.; Lagache, G.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Remazeilles, M.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France.
   [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Ducout, A.; Elsner, F.; Hivon, E.; Mangilli, A.; Moneti, A.; Prunet, S.; Sutter, P.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
   [Popa, L.] Inst Space Sci, Bucharest 077125, Romania.
   [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
   [Bridges, M.; Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
   [Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
   [Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife 38200, Spain.
   [Barreiro, R. B.; Bonavera, L.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain.
   [Bartlett, J. G.; Bock, J. J.; Colombo, L. P. L.; Dore, O.; Gorski, K. M.; Hanson, D.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Roudier, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Bonaldi, A.; Davies, R. D.; Davis, R. J.; Leahy, J. P.; Maffei, B.; Noviello, F.; Remazeilles, M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
   [Ashdown, M.; Bridges, M.; Challinor, A.; Gratton, S.; Harrison, D.; Migliaccio, M.; Stolyarov, V.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
   [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, CNRS, IN2P3, LAL, F-91383 Orsay, France.
   [Catalano, A.; Coulais, A.; Lamarre, J. -M.; Roudier, G.] CNRS, Observ Paris, LERMA, F-75014 Paris, France.
   [Arnaud, M.; Bobin, J.; Chamballu, A.; Marshall, D. J.; Pratt, G. W.; Starck, J. -L.; Sureau, F.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France.
   [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France.
   [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France.
   [Catalano, A.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Inst Natl Polytech Grenoble, CNRS IN2P3, Lab Phys Subatom & Cosmol, F-38026 St Martin Dheres, France.
   [Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France.
   [Kisner, T. S.] CNRS, F-91405 Orsay, France.
   [Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.; Sunyaev, R.; White, S. D. M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
   [Hanson, D.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
   [Tuovinen, J.; Varis, J.] McGill Univ, McGill Phys, Montreal, PQ H3A 2T8, Canada.
   [Murphy, J. A.] VTT Tech Res Ctr, MilliLab, Espoo 02044, Finland.
   [Christensen, P. R.; Naselsky, P.; Novikov, I.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland.
   [Crill, B. P.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
   [Savini, G.] CALTECH, Observat Cosmol, Pasadena, CA 91125 USA.
   [Lesgourgues, J.] UCL, Opt Sci Lab, London, England.
   [Baccigalupi, C.; Bielewicz, P.; Danese, L.; Gonzalez-Nuevo, J.; Paci, F.; Perrotta, F.; Renzi, A.] Ecole Polytech Fed Lausanne, SB ITP LPPC, CH-1015 Lausanne, Switzerland.
   [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
   [Moss, A.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
   [Sunyaev, R.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
   [Borrill, J.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia.
   [Stolyarov, V.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Church, S.; Osborne, S.] Russian Acad Sci, Special Astrophys Observ, Karachai Cherkessian 369167, Russia.
   [Armitage-Caplan, C.; Dunkley, J.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
   [Lesgourgues, J.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England.
   [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Delouis, J. -M.; Elsner, F.; Hivon, E.; Prunet, S.; Wandelt, B. D.] CERN, Div Theory, PH TH, CH-1211 Geneva 23, Switzerland.
   [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Paris 06, UMR7095, F-75014 Paris, France.
   [Battaner, E.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
   [Gorski, K. M.] Univ Granada, Dept Fis Teor & Cosmos, Fac Ciencias, E-18071 Granada, Spain.
   Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Bartolo, N (reprint author), Univ Padua, Dipartimento Fis & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy.
EM nicola.bartolo@pd.infn.it
RI Barreiro, Rita Belen/N-5442-2014; Butler, Reginald/N-4647-2015; Herranz,
   Diego/K-9143-2014; Vielva, Patricio/F-6745-2014; Toffolatti,
   Luigi/K-5070-2014; bonavera, laura/E-9368-2017; Remazeilles,
   Mathieu/N-1793-2015; Martinez-Gonzalez, Enrique/E-9534-2015;
   Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015;
   Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015;
   Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016;
   Kurki-Suonio, Hannu/B-8502-2016; Lahteenmaki, Anne/L-5987-2013; Tomasi,
   Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo,
   Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012;
   Piacentini, Francesco/E-7234-2010; Atrio-Barandela,
   Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Yvon,
   Dominique/D-2280-2015; 
OI Pierpaoli, Elena/0000-0002-7957-8993; Lilje, Per/0000-0003-4324-7794;
   Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi,
   Silvia/0000-0001-5105-1439; Valenziano, Luca/0000-0002-1170-0104;
   Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840;
   Paoletti, Daniela/0000-0003-4761-6147; Savini,
   Giorgio/0000-0003-4449-9416; Juvela, Mika/0000-0002-5809-4834; Villa,
   Fabrizio/0000-0003-1798-861X; Hivon, Eric/0000-0003-1880-2733; Starck,
   Jean-Luc/0000-0003-2177-7794; Franceschi, Enrico/0000-0002-0585-6591;
   Mitra, Sanjit/0000-0002-0800-4626; Galeotta,
   Samuele/0000-0002-3748-5115; Ricciardi, Sara/0000-0002-3807-4043;
   Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger,
   Kevin/0000-0001-7109-0099; Bouchet, Francois/0000-0002-8051-2924;
   TERENZI, LUCA/0000-0001-9915-6379; Matarrese,
   Sabino/0000-0002-2573-1243; Pasian, Fabio/0000-0002-4869-3227; WANDELT,
   Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272;
   Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785;
   Polenta, Gianluca/0000-0003-4067-9196; Butler,
   Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375;
   Herranz, Diego/0000-0003-4540-1417; Vielva,
   Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386;
   bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose
   Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595;
   de Bernardis, Paolo/0000-0001-6547-6446; Morgante,
   Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266;
   Maris, Michele/0000-0001-9442-2754; Martinez-Gonzalez,
   Enrique/0000-0002-0179-8590; Gonzalez-Nuevo,
   Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070;
   Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita,
   Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748;
   Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi,
   Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati,
   Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327;
   Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov,
   Vladislav/0000-0001-8151-828X; Burigana, Carlo/0000-0002-3005-5796;
   Zacchei, Andrea/0000-0003-0396-1192
NR 282
TC 1126
Z9 1126
U1 23
U2 87
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 NOV
PY 2014
VL 571
AR A24
DI 10.1051/0004-6361/201321554
PG 58
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT9ZK
UT WOS:000345282600018
ER

PT J
AU Montabone, L
   Marsh, K
   Lewis, SR
   Read, PL
   Smith, MD
   Holmes, J
   Spiga, A
   Lowe, D
   Pamment, A
AF Montabone, L.
   Marsh, K.
   Lewis, S. R.
   Read, P. L.
   Smith, M. D.
   Holmes, J.
   Spiga, A.
   Lowe, D.
   Pamment, A.
TI The Mars Analysis Correction Data Assimilation (MACDA) Dataset V1.0
SO GEOSCIENCE DATA JOURNAL
LA English
DT Article
DE mars atmosphere; mars reanalysis; mars Global Surveyor; global climate
   model (GCM); data assimilation
ID GENERAL-CIRCULATION MODEL; INTERANNUAL VARIABILITY; MARTIAN ATMOSPHERE;
   THERMAL STRUCTURE; DUST STORM; MGS TES; AEROSOL; SURFACE; SCHEME; VIKING
AB The Mars Analysis Correction Data Assimilation (MACDA) dataset version 1.0 contains the reanalysis of fundamental atmospheric and surface variables for the planet Mars covering a period of about three Martian years (a Martian year is about 1.88 terrestrial years). This has been produced by data assimilation of observations from NASA's Mars Global Surveyor (MGS) spacecraft during its science mapping phase (February 1999-August 2004). In particular, we have used retrieved thermal profiles and total dust optical depths from the Thermal Emission Spectrometer (TES) on board MGS. Data have been assimilated into a Mars global climate model (MGCM) using the Analysis Correction scheme developed at the UK Meteorological Office. The MGCM used is the UK spectral version of the Laboratoire de Meteorologie Dynamique (LMD, Paris, France) MGCM. MACDA is a joint project of the University of Oxford and The Open University in the UK.
C1 [Montabone, L.; Read, P. L.] Univ Oxford, Dept Phys, Oxford OX1 3PU, England.
   [Montabone, L.; Spiga, A.] Univ Paris 06, Meteorol Dynam Lab, Paris, France.
   [Marsh, K.; Lowe, D.; Pamment, A.] Rutherford Appleton Lab, STFC, London, England.
   [Lewis, S. R.; Holmes, J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
   [Smith, M. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Montabone, L (reprint author), Univ Oxford, Dept Phys, Parks Rd, Oxford OX1 3PU, England.
EM montabone@atm.ox.ac.uk
RI Spiga, Aymeric/O-4858-2014
OI Spiga, Aymeric/0000-0002-6776-6268
FU UK Science and Technology Facilities Council; UK Space Agency
   [ST/I001948/1, ST/K00106X/1, ST/J001597/1, ST/I003096/1]
FX MGS/TES retrievals of thermal profiles and infrared total dust optical
   depths have been provided by Michael D. Smith (NASA Goddard Space Flight
   Center, Greenbelt, MD, USA) to the University of Oxford in 2005. The
   MACDA reanalysis has been processed by the University of Oxford,
   Department of Physics, and The Open University, Department of Physical
   Sciences, in the UK. The reanalysis data files were provided to the
   British Atmospheric Data Centre in August 2011. L. Montabone wishes to
   thank Russell Jones at the University of Oxford for his invaluable help
   in setting up the MACDA web plotter tool, as well as Giacomo Correnti
   for useful tips in html and python programming. The authors are
   extremely grateful to J.-B. Madeleine and to another anonymous reviewer
   for their very useful comments, which helped to improve the paper. L.
   Montabone and S. R. Lewis wish also to acknowledge support from the UK
   Science and Technology Facilities Council and the UK Space Agency during
   the course of this work (Grant Refs. ST/I001948/1, ST/K00106X/1,
   ST/J001597/1, ST/I003096/1). Last but not the least; special thanks are
   due to BADC for supporting the MACDA v1.0 dataset.
NR 27
TC 16
Z9 16
U1 2
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2049-6060
J9 GEOSCI DATA J
JI Geosci. Data J.
PD NOV
PY 2014
VL 1
IS 2
BP 129
EP 139
DI 10.1002/gdj3.13
PG 11
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences
SC Geology; Meteorology & Atmospheric Sciences
GA CV4ES
UT WOS:000364219800004
ER

PT J
AU Nair, AK
   Kriz, RD
   Prosser, WH
AF Nair, Arun K.
   Kriz, Ronald D.
   Prosser, William H.
TI Nonlinear elastic effects in graphite/epoxy: An analytical and numerical
   prediction of energy flux deviation
SO WAVE MOTION
LA English
DT Article
DE Acoustoelastic effects; Composite material; Energy flux deviation;
   Stress induced anisotropy; Finite element method
ID WAVE-PROPAGATION; STRESS; VELOCITIES
AB Manipulating acoustic wave propagation through a material have several interdisciplinary applications. Here we predict shift in energy flux deviation for acoustic waves propagating in unidirectional graphite/epoxy due to applied normal and shear stresses using both an analytical model, using acoustoelastic continuum theory, and a finite element discrete numerical model. The acoustoelastic theory predicts that the quasi-transverse (QT) wave exhibits larger shifts in energy flux deviation compared to quasi-longitudinal (QL) or the pure transverse (PT) due to an applied shear stress for fiber orientation angle ranging from 0 degrees to 60 degrees. Due to an applied shear stress the QT wave exhibits a shift in energy flux deviation at 0 degrees fiber orientation angle as compared to normal stress case where the flux deviation and its load induced shift are both zero. A finite element model (FEM) is developed where equations of motion include the effect of nonlinear elastic coefficients. Element equations were integrated in time using Newmark's method to determine the shift in energy flux deviations in graphite/epoxy for different loading cases. The energy flux shift of QT waves predicted by FEM for fiber orientation angles from 0 degrees to 60 degrees for applied shear stress case is in excellent agreement with acoustoelastic theory. Because energy shift magnitudes are not small, it is possible to experimentally measure these shifts and calibrate shifts with respect to load type (normal/shear) and magnitude. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Nair, Arun K.; Kriz, Ronald D.] Virginia Tech, Dept Engn Sci & Mech, Blacksburg, VA 24061 USA.
   [Prosser, William H.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Nair, AK (reprint author), Univ Arkansas, Dept Mech Engn, 863 West Dickson St, Fayetteville, AR 72701 USA.
EM nair@uark.edu
OI Nair, Arun/0000-0003-2144-5335
FU Department of Mechanical Engineering, University of Arkansas
FX AKN and RDK would like to thank Advanced Research Computing at Virginia
   Tech for support with High Performance Computing. AKN would like to
   acknowledge support from the Department of Mechanical Engineering,
   University of Arkansas.
NR 31
TC 0
Z9 0
U1 1
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0165-2125
EI 1878-433X
J9 WAVE MOTION
JI Wave Motion
PD NOV
PY 2014
VL 51
IS 7
BP 1138
EP 1148
DI 10.1016/j.wavemoti.2014.06.002
PG 11
WC Acoustics; Mechanics; Physics, Multidisciplinary
SC Acoustics; Mechanics; Physics
GA AQ1MJ
UT WOS:000342545200008
ER

PT J
AU Bednarcyk, BA
   Aboudi, J
   Arnold, SM
AF Bednarcyk, Brett A.
   Aboudi, Jacob
   Arnold, Steven M.
TI The effect of general statistical fiber misalignment on predicted damage
   initiation in composites
SO COMPOSITES PART B-ENGINEERING
LA English
DT Article
DE Micro-mechanics; Strength; Directional orientation; Analytical
   modelling; High-Fidelity Generalized Method of Cells
ID RUBBER-LIKE MATERIALS; MICRO-MACRO APPROACH; COMPRESSIVE FAILURE; SPHERE
   MODEL; STRENGTH; MICROMECHANICS; NANOCOMPOSITES; IDENTIFICATION;
   ELASTICITY; WAVINESS
AB A micromechanical method is employed for the prediction of unidirectional composites in which the fiber orientation can possess various statistical misalignment distributions. The method relies on the probability-weighted averaging of the appropriate concentration tensors, which are established by the micromechanical procedure. This approach provides access to the local field quantities throughout the constituents, from which initiation of damage in the composite can be predicted. In contrast, a typical macromechanical procedure can determine the effective composite elastic properties in the presence of statistical fiber misalignment, but cannot provide the local fields. Fully random fiber distribution is presented as a special case using the proposed micromechanical method. Results are given that illustrate the effects of various amounts of fiber misalignment in terms of the standard deviations of in-plane and out-of-plane misalignment angles, where normal distributions have been employed. Damage initiation envelopes, local fields, effective moduli, and strengths are predicted for polymer and ceramic matrix composites with given normal distributions of misalignment angles, as well as fully random fiber orientation. Published by Elsevier Ltd.
C1 [Bednarcyk, Brett A.; Arnold, Steven M.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
   [Aboudi, Jacob] Tel Aviv Univ, IL-69978 Tel Aviv, Israel.
RP Bednarcyk, BA (reprint author), NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Brett.A.Bednarcyk@nasa.gov
NR 40
TC 8
Z9 8
U1 4
U2 19
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1359-8368
EI 1879-1069
J9 COMPOS PART B-ENG
JI Compos. Pt. B-Eng.
PD NOV
PY 2014
VL 66
BP 97
EP 108
DI 10.1016/j.compositesb.2014.04.014
PG 12
WC Engineering, Multidisciplinary; Materials Science, Composites
SC Engineering; Materials Science
GA AP7HD
UT WOS:000342247500011
ER

PT J
AU Shin, S
   Noh, YM
   Lee, K
   Lee, H
   Muller, D
   Kim, YJ
   Kim, K
   Shin, D
AF Shin, Sungkyun
   Noh, Young Min
   Lee, Kwonho
   Lee, Hanlim
   Mueller, Detlef
   Kim, Y. J.
   Kim, Kwanchul
   Shin, Dongho
TI Retrieval of the single scattering albedo of Asian dust mixed with
   pollutants using lidar observations
SO ADVANCES IN ATMOSPHERIC SCIENCES
LA English
DT Article
DE lidar; Asian dust; depolarization ratio; microphysical properties;
   single scattering albedo
ID MULTIWAVELENGTH RAMAN LIDAR; MICROPHYSICAL PARTICLE PARAMETERS; AEROSOL
   OPTICAL-PROPERTIES; BACKSCATTER LIDAR; AIRCRAFT MEASUREMENTS;
   CHEMICAL-COMPOSITION; POLLUTION AEROSOLS; SIZE DISTRIBUTION; NORTHEAST
   ASIA; KOREA
AB The vertical distribution of single scattering albedos (SSAs) of Asian dust mixed with pollutants was derived using the multi-wavelength Raman lidar observation system at Gwangju (35.10A degrees N, 126.53A degrees E). Vertical profiles of both backscatter and extinction coefficients for dust and non-dust aerosols were extracted from a mixed Asian dust plume using the depolarization ratio from lidar observations. Vertical profiles of backscatter and extinction coefficients of non-dust particles were input into an inversion algorithm to retrieve the SSAs of non-dust aerosols. Atmospheric aerosol layers at different heights had different light-absorbing characteristics. The SSAs of non-dust particles at each height varied with aerosol type, which was either urban/industrial pollutants from China transported over long distances at high altitude, or regional/local pollutants from the Korean peninsula. Taking advantage of independent profiles of SSAs of non-dust particles, vertical profiles of SSAs of Asian dust mixed with pollutants were estimated for the first time, with a new approach suggested in this study using an empirical determination of the SSA of pure dust. The SSAs of the Asian dust-pollutants mixture within the planetary boundary layer (PBL) were in the range 0.88-0.91, while the values above the PBL were in the range 0.76-0.87, with a very low mean value of 0.76 +/- 0.05. The total mixed dust plume SSAs in each aerosol layer were integrated over height for comparison with results from the Aerosol Robotics Network (AERONET) measurements. Values of SSA retrieved from lidar observations of 0.92 +/- 0.01 were in good agreement with the results from AERONET measurements.
C1 [Shin, Sungkyun; Noh, Young Min; Mueller, Detlef; Kim, Y. J.; Kim, Kwanchul; Shin, Dongho] Gwangju Inst Sci & Technol, Sch Environm Sci & Engn, Kwangju, South Korea.
   [Mueller, Detlef] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Houston, TX USA.
   [Lee, Kwonho] Kyungil Univ, Deta Geoinformat Engn, Taegu, South Korea.
   [Lee, Hanlim] Pukyong Natl Univ, Dept Spatial Informat Engn, Pusan, South Korea.
RP Noh, YM (reprint author), Gwangju Inst Sci & Technol, Sch Environm Sci & Engn, Kwangju, South Korea.
EM nym@gist.ac.kr
RI MUELLER, DETLEF/F-1010-2015; 
OI MUELLER, DETLEF/0000-0002-0203-7654; Kim, Kwanchul/0000-0002-7440-6703;
   Lee, Kwon-Ho/0000-0002-0844-5245
FU Korea Meteorological Administration Research and Development Program
   [CATER 2012-7080]; National Research Foundation of Korea (NRF) - Korean
   government (MEST) [2012R1A1A2002983]; National Research Foundation of
   Korea
FX This work was funded by the Korea Meteorological Administration Research
   and Development Program (Grant No. CATER 2012-7080). This work was also
   supported by a National Research Foundation of Korea (NRF) grant funded
   by the Korean government (MEST) (Grant No. 2012R1A1A2002983). Sungkyun
   SHIN is supported by the Global Ph.D. Fellowship program sponsored by
   the National Research Foundation of Korea.
NR 51
TC 3
Z9 3
U1 1
U2 19
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 NOV
PY 2014
VL 31
IS 6
BP 1417
EP 1426
DI 10.1007/s00376-014-3244-y
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AP2MW
UT WOS:000341907500016
ER

PT J
AU Poulain, X
   Benzerga, AA
   Goldberg, RK
AF Poulain, X.
   Benzerga, A. A.
   Goldberg, R. K.
TI Finite-strain elasto-viscoplastic behavior of an epoxy resin:
   Experiments and modeling in the glassy regime
SO INTERNATIONAL JOURNAL OF PLASTICITY
LA English
DT Article
DE Constitutive behavior; Amorphous polymers; Viscoplastic material; Finite
   strain; Mechanical testing
ID CONSTITUTIVE MODEL; AMORPHOUS POLYMERS; MECHANICAL-BEHAVIOR; SOLID
   POLYMERS; DEFORMATION; STRESS; TEMPERATURE; IMPLEMENTATION;
   LOCALIZATION; TENSION
AB The finite deformation response of an epoxy resin is investigated in the glassy regime using a constitutive relation that accounts for thermally activated yielding, pressure-sensitivity, strain softening and molecular chain reorientation. A previous formulation of this macromolecular model is modified so as to decouple the onset of yielding from the peak nominal stress, and enable accurate modeling of temperature and strain-rate effects concurrently. The latter cannot be modeled adequately with existing models when the temperature dependence of elastic moduli is accounted for. Tension and compression experiments are carried out on Epon 862 across a range of temperatures and strain rates. Special care is taken to extract the intrinsic material behavior from the recorded mechanical responses using a new technique of video-based extensometry, which is well adapted to cylindrical geometries. Key features of the data include a temperature dependence of elastic moduli and a tension-compression asymmetry that goes beyond differences in peak yield. The experimental data is divided in two sets for model calibration and assessment. The first set contains sufficient data to identify all model parameters following a procedure outlined in the paper. The second data set is used to assess the predictive capabilities of the model for test conditions not used in the calibration step. It is shown that when the tension and compression cases are treated separately, with respect to post-peak softening, model predictions are excellent over the investigated ranges of temperature and strain rate. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Poulain, X.; Benzerga, A. A.] Texas A&M Univ, Dept Aerosp Engn, College Stn, TX 77843 USA.
   [Benzerga, A. A.] Texas A&M Univ, Dept Mat Sci & Engn, College Stn, TX 77843 USA.
   [Goldberg, R. K.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Benzerga, AA (reprint author), Texas A&M Univ, Dept Aerosp Engn, College Stn, TX 77843 USA.
EM benzerga@tamu.edu
RI Benzerga, Amine/K-2045-2014
OI Benzerga, Amine/0000-0002-6644-470X
FU NASA Glenn Research Center [NNX07AV39A]; NSF International Institute for
   Multifunctional Materials for Energy Conversion (IIMEC) under DMR
   [0844082]
FX The authors acknowledge support from NASA Glenn Research Center under
   cooperative agreement NNX07AV39A and from the NSF International
   Institute for Multifunctional Materials for Energy Conversion (IIMEC)
   under DMR Grant# 0844082.
NR 33
TC 11
Z9 11
U1 3
U2 24
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0749-6419
EI 1879-2154
J9 INT J PLASTICITY
JI Int. J. Plast.
PD NOV
PY 2014
VL 62
BP 138
EP 161
DI 10.1016/j.ijplas.2014.07.002
PG 24
WC Engineering, Mechanical; Materials Science, Multidisciplinary; Mechanics
SC Engineering; Materials Science; Mechanics
GA AP7JO
UT WOS:000342253800009
ER

PT J
AU Sun, WB
   Lin, B
   Baize, RR
   Videen, G
   Hu, YX
AF Sun, Wenbo
   Lin, Bing
   Baize, Rosemary R.
   Videen, Gorden
   Hu, Yongxiang
TI Sensing Hadley cell with space-borne lidar
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Expansion of Hadley cell; Uppermost super-thin clouds; Climate;
   Space-borne lidar
ID CLOUDS; CIRRUS; TROPOPAUSE; MISSION; MODIS; CERES
AB Some recent studies reported expansion of the Earth's tropical regime in the past few decades. The poleward expansion of the Hadley cell is a strong indication of the warming of the globe. The extent of Hadley cell also has very important implications to the climate of dry subtropical regions because of the prevalence of precipitation in the deep tropical belt. Determination of the Hadley circulation especially its extent has great significance for monitoring global climate change and for the subtropical climate studies. Although many methods have been developed in recent years, reliable measurement of the extent of Hadley cell is still an issue in climate studies. This letter shows that the extent of the Hadley cell could reliably be estimated by measuring the height of the uppermost super-thin clouds in the troposphere with space-borne lidar. Through consecutive multi-year measurements of the height of the uppermost super-thin clouds, a good estimation of the expansion of the Hadley cell could be obtained. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Sun, Wenbo] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
   [Sun, Wenbo; Lin, Bing; Baize, Rosemary R.; Hu, Yongxiang] NASA Langley Res Ctr, Hampton, VA 23681 USA.
   [Videen, Gorden] Space Sci Inst, Boulder, CO 80301 USA.
   [Videen, Gorden] Army Res Lab, Adelphi, MD 20783 USA.
RP Sun, WB (reprint author), NASA Langley Res Ctr, Mail Stop 420,21 Langley Blvd, Hampton, VA 23681 USA.
EM wenbo.sun-1@nasa.gov
RI Hu, Yongxiang/K-4426-2012; Richards, Amber/K-8203-2015
FU NASA Glory fund [09-GLORY09-0027]; NASA CLARREO Mission
FX This work was supported by NASA Glory fund 09-GLORY09-0027 and also
   partially supported by NASA CLARREO Mission. The authors thank Hal B.
   Maring, Michael I. Mishchenko, Bruce A. Wielicki, and David F. Young for
   these supports.
NR 26
TC 1
Z9 1
U1 0
U2 16
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 NOV
PY 2014
VL 148
BP 38
EP 41
DI 10.1016/j.jqsrt.2014.06.017
PG 4
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AP7JR
UT WOS:000342254100006
ER

PT J
AU Lamouroux, J
   Gamache, RR
   Schwenke, DW
AF Lamouroux, J.
   Gamache, R. R.
   Schwenke, D. W.
TI Determination of the reduced matrix elements using accurate ab initio
   wavefunctions: Formalism and its application to the vibrational ground
   state (000) of (H2O)-O-16
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Water vapor; Wavefunctions; Reduced matrix elements; Sum rules
ID NONLOCAL THERMODYNAMIC-EQUILIBRIUM; MOLECULAR SPECTROSCOPIC DATABASE;
   ROVIBRATIONAL ENERGY-LEVELS; N-2-BROADENED HALF-WIDTHS; ASYMMETRIC-TOP
   MOLECULES; SINGLE-SUM EXPRESSION; WATER-VAPOR; LEGENDRE POLYNOMIALS;
   TRIATOMIC-MOLECULES; INTERACTING STATES
AB The calculations of the reduced matrix elements for 441 rotational collisional transitions for rotational quantum numbers of the lower state up top J ''=20 in the vibrational ground state of (H2O)-O-16 are presented using effective and ab initio wavefunctions. Effective wavefunctions are derived from a Watson A-reduced Hamiltonian with the effective parameters determined by Matsushima et al. [Matsushima et al., J Mol Struct 1995;352-353:371]. The ab initio wavefunctions used in this study are from the work of Partridge and Schwenke [Partridge, H, Schwenke, DW. J Chem Phys 1997;106:4618]. The comparison of the reduced matrix elements obtained by both methods is described. It is demonstrated that, even for the rotational band, the effective wavefunctions show problems for some states. (C) 2014 Published by Elsevier Ltd.
C1 [Lamouroux, J.; Gamache, R. R.] Univ Massachusetts Lowell, Dept Environm Earth & Atmospher Sci, One Univ Ave, Lowell, MA 01854 USA.
   [Schwenke, D. W.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Gamache, RR (reprint author), Univ Massachusetts Lowell, Dept Environm Earth & Atmospher Sci, One Univ Ave, Lowell, MA 01854 USA.
EM Robert_Gamache@timl.edu
RI schwenke, david/I-3564-2013
FU National Science Foundation, USA [AGS-1156862]
FX JL and RRG are pleased to acknowledge support of this research by the
   National Science Foundation, USA through Grant no. AGS-1156862. 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.
NR 67
TC 0
Z9 0
U1 0
U2 3
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 NOV
PY 2014
VL 148
BP 49
EP 57
DI 10.1016/j.jqsrt.2014.06.011
PG 9
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AP7JR
UT WOS:000342254100008
ER

PT J
AU Loftus, AM
   Cotton, WR
   Carrio, GG
AF Loftus, A. M.
   Cotton, W. R.
   Carrio, G. G.
TI A triple-moment hail bulk microphysics scheme. Part I: Description and
   initial evaluation
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Hail; Microphysics; Numerical modeling
ID MIDLATITUDE SQUALL LINE; CONVECTIVE STORMS; NUMERICAL SIMULATIONS; CLOUD
   MICROPHYSICS; PARAMETERIZATION SCHEMES; SENSITIVITY EXPERIMENTS; PHASE
   MICROPHYSICS; MODEL DESCRIPTION; SIZE DISTRIBUTION; HAILSTONE GROWTH
AB Hail processes in deep convection can have a substantial impact on precipitation characteristics as well as on dynamic and thermodynamic properties of convective downdrafts and cold pools, yet the realistic representation of hail in many cloud-resolving models employing bulk microphysical schemes is challenging. The limits imposed by fixing one or two of the distribution parameters in many one- and two-moment bulk microphysics schemes often lead to particularly poor representations of particles within the tails of size distribution spectra; an especially important consideration for hail, which covers a broad range of sizes in nature. In order to improve the representation of hail distributions in simulations of deep moist convection in cloud-resolving numerical models, a new triple-moment bulk hail microphysics scheme (3MHAIL) is presented and evaluated. The 3MHAIL scheme predicts the relative dispersion parameter for a gamma distribution function via prognostication of the sixth moment (related to the reflectivity factor) of the distribution in addition to the mass mixing ratio and number concentration (third and zeroeth moments, respectively) thereby allowing for a fully prognostic distribution function. Significant improvement in the representation of sedimentation, melting, and formation processes of hail are achieved with the 3MHAIL scheme compared to lower-order moment schemes. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Loftus, A. M.; Cotton, W. R.; Carrio, G. G.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
RP Loftus, AM (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM adrian.m.loftus@nasa.gov
FU National Science Foundation [ATM-0324324, ATM-0638910, AGS-1005041]
FX The authors wish to thank Steve Saleeby and Bob Walko for assistance
   with the RAMS model code, as well as Jason Milbrandt and one anonymous
   reviewer for their suggestions on improving the paper. This research was
   supported by the National Science Foundation grants ATM-0324324,
   ATM-0638910, and AGS-1005041.
NR 83
TC 10
Z9 10
U1 1
U2 12
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 NOV
PY 2014
VL 149
BP 35
EP 57
DI 10.1016/j.atmosres.2014.05.013
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AO6NF
UT WOS:000341468100004
ER

PT J
AU Tadesse, T
   Pevtsov, AA
   Wiegelmann, T
   MacNeice, PJ
   Gosain, S
AF Tadesse, Tilaye
   Pevtsov, Alexei A.
   Wiegelmann, T.
   MacNeice, P. J.
   Gosain, S.
TI Global Solar Free Magnetic Energy and Electric Current Density
   Distribution of Carrington Rotation 2124
SO SOLAR PHYSICS
LA English
DT Article
DE Active regions, magnetic fields; Active regions, models; Magnetic
   fields, corona; Magnetic fields, models; Magnetic fields, photosphere
ID FORCE-FREE FIELD; VECTOR MAGNETOGRAPH DATA; ACTIVE REGIONS; SPHERICAL
   GEOMETRY; QUIET-SUN; MODELS; RECONSTRUCTION; EXTRAPOLATION; EJECTIONS;
   STRENGTH
AB Solar eruptive phenomena, like flares and coronal mass ejections (CMEs), are governed by magnetic fields. To describe the structure of these phenomena one needs information on the magnetic flux density and the electric current density vector components in three dimensions throughout the atmosphere. However, current spectro-polarimetric measurements typically limit the determination of the vector magnetic field to only the photosphere. Therefore, there is considerable interest in accurate modeling of the solar coronal magnetic field using photospheric vector magnetograms as boundary data. In this work, we model the coronal magnetic field for global solar atmosphere using nonlinear force-free field (NLFFF) extrapolation codes implemented to a synoptic maps of photospheric vector magnetic field synthesized from the Vector Spectromagnetograph (VSM) on Synoptic Optical Long-term Investigations of the Sun (SOLIS) as boundary condition. Using the resulting three-dimensional magnetic field, we calculate the three-dimensional electric current density and magnetic energy throughout the solar atmosphere for Carrington rotation 2124 using our global extrapolation code. We found that spatially, the low-lying, current-carrying core field demonstrates a strong concentration of free energy in the active-region core, from the photosphere to the lower corona (about 70 Mm). The free energy density appears largely co-spatial with the electric current distribution.
C1 [Tadesse, Tilaye; MacNeice, P. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Pevtsov, Alexei A.; Gosain, S.] Natl Solar Observ, Sunspot, NM 88349 USA.
   [Wiegelmann, T.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
RP Tadesse, T (reprint author), NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA.
EM tilaye.tadesse.asfaw@nasa.gov; apevtsov@nso.edu; wiegelmann@mps.mpg.de;
   peter.j.macneice@nasa.gov; sgosain@nso.edu
OI Pevtsov, Alexei/0000-0003-0489-0920
FU NASA
FX The authors thank the anonymous referee for helpful and detailed
   comments. Data are courtesy of NASA/SDO and the AIA and HMI science
   teams. This work utilizes SOLIS data obtained by the NSO Integrated
   Synoptic Program (NISP), managed by the National Solar Observatory,
   which is operated by the Association of Universities for Research in
   Astronomy (AURA), Inc. under a cooperative agreement with the National
   Science Foundation. This research was supported by an appointment to the
   NASA Postdoctoral Program at the Goddard Space Flight Center (GSFC),
   administered by Oak Ridge Associated Universities through a contract
   with NASA.
NR 53
TC 3
Z9 3
U1 0
U2 13
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 NOV
PY 2014
VL 289
IS 11
BP 4031
EP 4045
DI 10.1007/s11207-014-0581-z
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO6YW
UT WOS:000341499800002
ER

PT J
AU Webber, SAH
   Karna, N
   Pesnell, WD
   Kirk, MS
AF Webber, S. A. Hess
   Karna, N.
   Pesnell, W. D.
   Kirk, M. S.
TI Areas of Polar Coronal Holes from 1996 Through 2010
SO SOLAR PHYSICS
LA English
DT Article
DE Coronal holes; Solar cycle, observations; Corona, quiet
ID IMAGING TELESCOPE; MAGNETIC-FIELD; CYCLE 23; SOLAR; SUNSPOT; EUV;
   EVOLUTION; REVERSAL; MAXIMUM; PREDICT
AB Polar coronal holes (PCHs) trace the magnetic variability of the Sun throughout the solar cycle. Their size and evolution have been studied as proxies for the global magnetic field. We present measurements of the PCH areas from 1996 through 2010, derived from an updated perimeter-tracing method and two synoptic-map methods. The perimeter-tracing method detects PCH boundaries along the solar limb, using full-disk images from the SOlar and Heliospheric Observatory/Extreme ultraviolet Imaging Telescope (SOHO/EIT). One synoptic-map method uses the line-of-sight magnetic field from the SOHO/Michelson Doppler Imager (MDI) to determine the unipolarity boundaries near the poles. The other method applies thresholding techniques to synoptic maps created from EUV image data from EIT. The results from all three methods suggest that the solar maxima and minima of the two hemispheres are out of phase. The maximum PCH area, averaged over the methods in each hemisphere, is approximately 6 % during both solar minima spanned by the data (between Solar Cycles 22/23 and 23/24). The northern PCH area began a declining trend in 2010, suggesting a downturn toward the maximum of Solar Cycle 24 in that hemisphere, while the southern hole remained large throughout 2010.
C1 [Webber, S. A. Hess; Karna, N.; Pesnell, W. D.; Kirk, M. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Webber, S. A. Hess; Karna, N.] George Mason Univ, Fairfax, VA 22030 USA.
RP Pesnell, WD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM shessweb@masonlive.gmu.edu; nkarna@masonlive.gmu.edu;
   william.d.pesnell@nasa.gov; michael.s.kirk@nasa.gov
RI Pesnell, William/D-1062-2012; 
OI Pesnell, William/0000-0002-8306-2500; Hess Webber, Shea
   A/0000-0002-3631-6491
FU NASA's Solar Dynamics Observatory (SDO); Fredrick Bruhweiler; Catholic
   University of America; Schlumberger Foundation Faculty for the Future;
   NASA
FX This work was supported by NASA's Solar Dynamics Observatory (SDO). S.
   A. Hess Webber thanks Fredrick Bruhweiler and the Catholic University of
   America for their support. N. Karna thanks the Schlumberger Foundation
   Faculty for the Future for supporting the research. The authors thank
   Arthur Poland for making suggestions that improved the discussion. The
   EIT images are courtesy of the SOHO/EIT consortium at
   umbra.nascom.nasa.gov/eit/. The MDI images are provided by the Solar
   Oscillations Investigation (SOI) team of the Stanford-Lockheed Institute
   for Space Research. The MDI magnetic synoptic-map data and description
   can be accessed at soi.stanford.edu/magnetic/index6.html. SOHO is a
   mission of international cooperation between ESA and NASA. The MDI
   magnetogram data can be found at soi.stanford.edu/magnetic/index5.html.
   Wilcox Solar Observatory data used in this study were obtained from
   wso.stanford.edu/Polar.html, courtesy of J.T. Hoeksema. The Wilcox Solar
   Observatory is currently supported by NASA. The timing and values of
   solar-cycle extrema were obtained from
   www.ngdc.noaa.gov/stp/space-weather/solar-data/solar-indices/sunspot-num
   bers/cycle-data/table_cycle-dates_maximum-minimum.txt. The EIT and AIA
   synoptic maps constructed for use in this research can be found at
   spaceweather.gmu.edu/projects/synop/.
NR 33
TC 7
Z9 7
U1 0
U2 7
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 NOV
PY 2014
VL 289
IS 11
BP 4047
EP 4067
DI 10.1007/s11207-014-0564-0
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO6YW
UT WOS:000341499800003
ER

PT J
AU Webb, DF
   Bisi, MM
   de Koning, CA
   Farrugia, CJ
   Jackson, BV
   Jian, LK
   Lugaz, N
   Marubashi, K
   Mostl, C
   Romashets, EP
   Wood, BE
   Yu, HS
AF Webb, D. F.
   Bisi, M. M.
   de Koning, C. A.
   Farrugia, C. J.
   Jackson, B. V.
   Jian, L. K.
   Lugaz, N.
   Marubashi, K.
   Moestl, C.
   Romashets, E. P.
   Wood, B. E.
   Yu, H. -S.
TI An Ensemble Study of a January 2010 Coronal Mass Ejection (CME):
   Connecting a Non-obvious Solar Source with Its ICME/Magnetic Cloud
SO SOLAR PHYSICS
LA English
DT Article
ID MAGNETIC-FLUX ROPE; EMPIRICAL RECONSTRUCTION; STEREO MISSION;
   CONSTANT-ALPHA; SOHO MISSION; IMAGER SMEI; WIND; MODEL; EARTH; LASCO
AB A distinct magnetic cloud (MC) was observed in-situ at the Solar TErrestrial RElations Observatory (STEREO)-B on 20 -aEuro parts per thousand 21 January 2010. About three days earlier, on 17 January, a bright flare and coronal mass ejection (CME) were clearly observed by STEREO-B, which suggests that this was the progenitor of the MC. However, the in-situ speed of the event, several earlier weaker events, heliospheric imaging, and a longitude mismatch with the STEREO-B spacecraft made this interpretation unlikely. We searched for other possible solar eruptions that could have caused the MC and found a faint filament eruption and the associated CME on 14 -aEuro parts per thousand 15 January as the likely solar source event. We were able to confirm this source by using coronal imaging from the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI)/EUVI and COR and Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronograph (LASCO) telescopes and heliospheric imaging from the Solar Mass Ejection Imager (SMEI) and the STEREO/Heliospheric Imager instruments. We use several empirical models to understand the three-dimensional geometry and propagation of the CME, analyze the in-situ characteristics of the associated ICME, and investigate the characteristics of the MC by comparing four independent flux-rope model fits with the launch observations and magnetic-field orientations. The geometry and orientations of the CME from the heliospheric-density reconstructions and the in-situ modeling are remarkably consistent. Lastly, this event demonstrates that a careful analysis of all aspects of the development and evolution of a CME is necessary to correctly identify the solar counterpart of an ICME/MC.
C1 [Webb, D. F.] Boston Coll, ISR, Chestnut Hill, MA 02167 USA.
   [Bisi, M. M.] Rutherford Appleton Lab, RAL Space Sci & Technol Facil Council, Oxford, England.
   [de Koning, C. A.] NOAA, Space Weather Predict Ctr, Boulder, CO USA.
   [de Koning, C. A.] Univ Colorado, CIRES, Boulder, CO 80309 USA.
   [Farrugia, C. J.; Lugaz, N.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
   [Farrugia, C. J.; Lugaz, N.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
   [Jackson, B. V.; Yu, H. -S.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
   [Jian, L. K.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
   [Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Marubashi, K.] Korea Astron & Space Sci Inst, Taejon, South Korea.
   [Moestl, C.] Graz Univ, Inst Phys, A-8010 Graz, Austria.
   [Moestl, C.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
   [Romashets, E. P.] Lone Star Coll, Houston, TX USA.
   [Wood, B. E.] Naval Res Lab, Div Space Sci, Washington, DC USA.
RP Webb, DF (reprint author), Boston Coll, ISR, Chestnut Hill, MA 02167 USA.
EM david.webb@bc.edu
RI Lugaz, Noe/C-1284-2008; Jian, Lan/B-4053-2010
OI Lugaz, Noe/0000-0002-1890-6156; Jian, Lan/0000-0002-6849-5527
FU Air Force at Boston College [AF19628-00-K-0073, FA8718-04-C-0006]; Navy
   contracts [N00173-07-1-G016, N00173-10-1-G001]; European Union [263252];
   Marie Curie International Outgoing Fellowship within the 7th European
   Community Framework Programme; UCSD NSF [AG-S-1053766, ATM-0925023];
   NASA [NNX11AB50G, NNX13AP39G, NAS5-00132]; AFOSR [11NE043]; NSF
   [AG-S-1242798, AG-S-1140211]; NASA's Science Mission Directorate as part
   of the STEREO project; STFC; NASA TRT grant [NNX09AJ84G]
FX We thank the Institute of Physics, University of Graz, Austria for
   hosting a workshop on this event in March 2011. We are grateful to the
   STEREO/SECCHI PI, Russell Howard, the STEREO/PLASTIC PI, Antoine Galvin,
   and the STEREO/IMPACT PI, Janet Luhmann, for the use of data and
   analyses from these instrument suites. We thank Gemma Attrill, John
   Clover, Timothy Howard, Nariaki Nitta, Dusan Odstrcil, S. James Tappin,
   and Marek Vandas for their analysis efforts on these events during the
   January 2010 period. The SMEI instrument is a collaborative project of
   the US Air Force Research Laboratory, NASA, the University of California
   at San Diego, the University of Birmingham, UK, Boston College, and
   Boston University. The STEREO/SECCHI Heliospheric Imager (HI) instrument
   was developed by a collaboration that included the Rutherford Appleton
   Laboratory and the University of Birmingham, both in the United Kingdom,
   the Centre Spatial de Liege (CSL), Belgium, and the US Naval Research
   Laboratory (NRL), Washington DC, USA. The SECCHI project is an
   international consortium of the Naval Research Laboratory, Lockheed
   Martin Solar and Astrophysics Lab, NASA Goddard Space Flight Center,
   Rutherford Appleton Laboratory, University of Birmingham,
   Max-Planck-Institut fur Sonnensystemforschung, Centre Spatial de Liege,
   Institut d'Optique Theorique et Appliquee, and Institut d'Astrophysique
   Spatiale. We also benefitted from data from the SOHO mission, which is
   an international collaboration between and ESA and NASA, and also from
   the SOHO/LASCO CME catalog, generated and maintained by the Center for
   Solar Physics and Space Weather, The Catholic University of America in
   cooperation with NRL and NASA. The work of DFW was supported at Boston
   College by Air Force contracts AF19628-00-K-0073 and FA8718-04-C-0006
   and Navy contracts N00173-07-1-G016 and N00173-10-1-G001. The work of CM
   was supported by the European Union Seventh Framework Programme
   (FP7/2007-2013) under grant agreement no. 263252 (COMESEP), and by a
   Marie Curie International Outgoing Fellowship within the 7th European
   Community Framework Programme. BVJ and H-SY were supported by UCSD NSF
   grant and AG-S-1053766, NASA grant NNX11AB50G, and AFOSR grant 11NE043.
   LKJ was supported by NSF grant AG-S-1242798 and by NASA's Science
   Mission Directorate as part of the STEREO project, including the IMPACT
   and PLASTIC investigations. MMB acknowledges support on these analyses
   initially from UCSD NSF grant ATM-0925023, and also from STFC funding to
   RAL Space at The Rutherford Appleton Laboratory. CJF was supported by
   NASA grant NNX13AP39G and NSF grant AG-S-1140211. Part of this work was
   supported by NASA (NAS5-00132) for STEREO/PLASTIC at UNH. CADK was
   supported by NASA TR&T grant NNX09AJ84G.
NR 84
TC 2
Z9 2
U1 0
U2 11
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 NOV
PY 2014
VL 289
IS 11
BP 4173
EP 4208
DI 10.1007/s11207-014-0571-1
PG 36
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO6YW
UT WOS:000341499800010
ER

PT J
AU Kobayashi, K
   Cirtain, J
   Winebarger, AR
   Korreck, K
   Golub, L
   Walsh, RW
   De Pontieu, B
   DeForest, C
   Title, A
   Kuzin, S
   Savage, S
   Beabout, D
   Beabout, B
   Podgorski, W
   Caldwell, D
   McCracken, K
   Ordway, M
   Bergner, H
   Gates, R
   McKillop, S
   Cheimets, P
   Platt, S
   Mitchell, N
   Windt, D
AF Kobayashi, Ken
   Cirtain, Jonathan
   Winebarger, Amy R.
   Korreck, Kelly
   Golub, Leon
   Walsh, Robert W.
   De Pontieu, Bart
   DeForest, Craig
   Title, Alan
   Kuzin, Sergey
   Savage, Sabrina
   Beabout, Dyana
   Beabout, Brent
   Podgorski, William
   Caldwell, David
   McCracken, Kenneth
   Ordway, Mark
   Bergner, Henry
   Gates, Richard
   McKillop, Sean
   Cheimets, Peter
   Platt, Simon
   Mitchell, Nick
   Windt, David
TI The High-Resolution Coronal Imager (Hi-C)
SO SOLAR PHYSICS
LA English
DT Article
DE Solar corona; Solar instrumentation; Solar imaging; Extreme ultraviolet
ID SOLAR CORONA; REGION; LOOPS; DYNAMICS; MOSS; RECONNECTION; HINODE;
   SKYLAB; ENERGY; SCALE
AB The High-Resolution Coronal Imager (Hi-C) was flown on a NASA sounding rocket on 11 July 2012. The goal of the Hi-C mission was to obtain high-resolution (a parts per thousand aEuro parts per thousand 0.3 -aEuro parts per thousand 0.4''), high-cadence (a parts per thousand aEuro parts per thousand 5 seconds) images of a solar active region to investigate the dynamics of solar coronal structures at small spatial scales. The instrument consists of a normal-incidence telescope with the optics coated with multilayers to reflect a narrow wavelength range around 19.3 nm (including the Fe xii 19.5-nm spectral line) and a 4096x4096 camera with a plate scale of 0.1''aEuro parts per thousand pixel(-1). The target of the Hi-C rocket flight was Active Region 11520. Hi-C obtained 37 full-frame images and 86 partial-frame images during the rocket flight. Analysis of the Hi-C data indicates the corona is structured on scales smaller than currently resolved by existing satellite missions.
C1 [Kobayashi, Ken] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA.
   [Kobayashi, Ken; Cirtain, Jonathan; Winebarger, Amy R.; Savage, Sabrina; Beabout, Dyana; Beabout, Brent] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
   [Korreck, Kelly; Golub, Leon; Podgorski, William; Caldwell, David; McCracken, Kenneth; Ordway, Mark; Bergner, Henry; Gates, Richard; McKillop, Sean; Cheimets, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Walsh, Robert W.; Platt, Simon; Mitchell, Nick] Univ Cent Lancashire, Preston PR1 2HE, Lancs, England.
   [De Pontieu, Bart; Title, Alan] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
   [DeForest, Craig] Southwest Res Inst, Boulder, CO 80302 USA.
   [Kuzin, Sergey] Russian Acad Sci, PN Lebedev Phys Inst, Moscow 119991, Russia.
   [Windt, David] Reflect Xray Opt LLC, New York, NY 10027 USA.
RP Kobayashi, K (reprint author), NASA, George C Marshall Space Flight Ctr, ZP 13, Huntsville, AL 35812 USA.
EM ken.kobayashi-1@nasa.gov
RI Kuzin, Sergey/M-3435-2015; 
OI Korreck, Kelly/0000-0001-6095-2490
FU NASA's Low Cost Access to Space program; Presidium of the RAS [22]
FX We acknowledge the High-Resolution Coronal Imager instrument grant
   funded by the NASA's Low Cost Access to Space program. MSFC/NASA led the
   mission and partners include the Smithsonian Astrophysical Observatory
   in Cambridge, MA, USA; Lockheed Martin's Solar Astrophysical Laboratory
   in Palo Alto, CA, USA; the University of Central Lancashire in
   Lancashire, England; and the Lebedev Physical Institute of the Russian
   Academy of Sciences in Moscow, Russia. LPI was supported by the Program
   no. 22 of the Presidium of the RAS.
NR 29
TC 19
Z9 19
U1 0
U2 6
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 NOV
PY 2014
VL 289
IS 11
BP 4393
EP 4412
DI 10.1007/s11207-014-0544-4
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO6YW
UT WOS:000341499800020
ER

PT J
AU Acar, E
   Karaca, HE
   Tobe, H
   Noebe, RD
   Chumlyakov, YI
AF Acar, E.
   Karaca, H. E.
   Tobe, H.
   Noebe, R. D.
   Chumlyakov, Y. I.
TI Orientation dependence of the shape memory properties in aged
   Ni45.3Ti29.7Hf20Pd5 single crystals
SO INTERMETALLICS
LA English
DT Article
DE Shape-memory effects; Martensitic transformations; Age-hardening;
   Mechanical testing; Shape-memory alloys
ID MARTENSITIC TRANSFORMATIONS; COMPRESSIVE RESPONSE; ALLOYS; BEHAVIOR;
   NITI; PHASE; SUBSTRUCTURE; STRENGTH
AB The shape memory properties of Ni45.3Ti29.7Hf20Pd5 single crystals aged at 550 degrees C for 3 h and at 600 degrees C for 48 h were investigated along the [111], [011] and [ 117] orientations in compression. The material was stronger along the [-117] orientation compared to the [111] and [011] orientations based on load-biased thermal cycling experiments. The shape memory properties such as reversible strain, temperature hysteresis, critical stress for stress-induced martensite transformation and Clausius-Clapeyron relations were also strong functions of orientation and aging condition (precipitate characteristics). Shape memory effect with no or negligible irrecoverable strain was observed under stress levels as high as 1000 MPa. After aging at 550 degrees C for 3 h, the maximum reversible strains were 2.2%, 2.7% and 0.7% along the [111], [011] and [ 117] orientations, respectively. Aging at 600 degrees C for 48 h resulted in maximum reversible strains of 2.3%, 3.2% and 0.9% along the [111], [011] and [-117] orientations, respectively. In both cases, similar levels of transformation strain, as a function of orientation, were observed during superelastic testing. The maximum work output reached 27 J/cm(3) in the [011] orientation after aging at 550 degrees C for 3 h. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Acar, E.; Karaca, H. E.; Tobe, H.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
   [Noebe, R. D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
   [Chumlyakov, Y. I.] Tomsk State Univ, Siberian Phys Tech Inst, Tomsk 634050, Russia.
   [Acar, E.] Erciyes Univ, TR-38039 Kayseri, Turkey.
RP Karaca, HE (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
EM karaca@engr.uky.edu
RI Chumlyakov, Yuriy/R-6496-2016
FU Turkish Ministry of Education; NASA Fundamental Aeronautics Program;
   Aeronautical Sciences Project; NASA EPSCOR Program [NNX11AQ31A]; KY
   EPSCoR RID Program [3049024332]; RFBR Project [10-03-0154-a]
FX We would like to thank the Turkish Ministry of Education for their
   financial support during this research. This work was supported in part
   by the NASA Fundamental Aeronautics Program, Aeronautical Sciences
   Project and the NASA EPSCOR Program under grant No: NNX11AQ31A, KY
   EPSCoR RID Program under grant No: 3049024332 and RFBR Project with
   grant No: 10-03-0154-a.
NR 33
TC 7
Z9 8
U1 7
U2 29
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0966-9795
EI 1879-0216
J9 INTERMETALLICS
JI Intermetallics
PD NOV
PY 2014
VL 54
BP 60
EP 68
DI 10.1016/j.intermet.2014.04.011
PG 9
WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy &
   Metallurgical Engineering
SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering
GA AO0FF
UT WOS:000340983800009
ER

PT J
AU Marshak, A
   Evans, KF
   Varnai, T
   Wen, GY
AF Marshak, Alexander
   Evans, K. Frank
   Varnai, Tamas
   Wen, Guoyong
TI Extending 3D near-cloud corrections from shorter to longer wavelengths
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Aerosol optical thickness; 3D spectral correction for longer
   wavelengths; Large-Eddy Simulations
ID AEROSOL OPTICAL-THICKNESS; CLEAR-AIR; MODIS; PRODUCTS; DEPTH;
   SIMULATIONS; SATELLITE; VICINITY; OCEAN; CERES
AB Satellite observations have shown a positive correlation between cloud amount and aerosol optical thickness (AOT) that can be explained by the humidification of aerosols near clouds, and/or by cloud contamination by sub-pixel size clouds and the cloud adjacency effect. The last effect may substantially increase reflected radiation in cloud-free columns, leading to overestimates in the retrieved AOT. For clear-sky areas near boundary layer clouds the main contribution to the enhancement of clear sky reflectance at shorter wavelengths comes from the radiation scattered into clear areas by clouds and then scattered to the sensor by air molecules. Because of the wavelength dependence of air molecule scattering, this process leads to a larger reflectance increase at shorter wavelengths, and can be corrected using a simple two-layer model [18]. However, correcting only for molecular scattering skews spectral properties of the retrieved AOT. Kassianov and Ovtchinnikov [9] proposed a technique that uses spectral reflectance ratios to retrieve AOT in the vicinity of clouds; they assumed that the cloud adjacency effect influences the spectral ratio between reflectances at two wavelengths less than it influences the reflectances themselves. This paper combines the two approaches: It assumes that the 3D correction for the shortest wavelength is known with some uncertainties, and then it estimates the 3D correction for longer wavelengths using a modified ratio method. The new approach is tested with 3D radiances simulated for 26 cumulus fields from Large-Eddy Simulations, supplemented with 40 aerosol profiles. The results showed that (i) for a variety of cumulus cloud scenes and aerosol profiles over ocean the 3D correction due to cloud adjacency effect can be extended from shorter to longer wavelengths and (ii) the 3D corrections for longer wavelengths are not very sensitive to unbiased random uncertainties in the 3D corrections at shorter wavelengths. Published by Elsevier Ltd.
C1 [Marshak, Alexander] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Evans, K. Frank] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
   [Varnai, Tamas] Univ Maryland Baltimore Cty, JCET, Baltimore, MD 21228 USA.
   [Wen, Guoyong] Morgan State Univ, GESTAR, Greenbelt, MD 20771 USA.
RP Marshak, A (reprint author), NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA.
EM alexander.marshak@nasa.gov
RI Marshak, Alexander/D-5671-2012
FU Office of Science, ASR program [DE-AI02-08ER64562]; NASA Radiation
   Sciences Program
FX This research was supported by the Office of Science (Biological and
   Environmental Research, US Department of Energy, Interagency Agreement
   no. DE-AI02-08ER64562) as part of the ASR program and by the NASA
   Radiation Sciences Program managed by Hal Mating. We also thank Drs.
   Robert Levy and Alexei Lyapustin for fruitful discussions, valuable
   comments, and suggestions.
NR 31
TC 5
Z9 7
U1 0
U2 10
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 NOV
PY 2014
VL 147
BP 79
EP 85
DI 10.1016/j.jqsrt.2014.05.022
PG 7
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AN6GY
UT WOS:000340694200010
ER

PT J
AU Huang, XC
   Gamache, RR
   Freedman, RS
   Schwenke, DW
   Lee, TJ
AF Huang, Xinchuan
   Gamache, Robert R.
   Freedman, Richard S.
   Schwenke, David W.
   Lee, Timothy J.
TI Reliable infrared line lists for 13 CO2 isotopologues up to E '=18,000
   cm(-1) and 1500 K, with line shape parameters
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Carbon dioxide (CO2); Isotopologues; IR line list; Line shape; Refined
   potential energy surface; Partition sum
ID RESOLUTION TRANSMISSION MEASUREMENTS; HALF-WIDTHS; SEMICLASSICAL
   CALCULATIONS; SPECTROSCOPIC DATABASE; 00001 BANDS; TRANSITIONS;
   COLLISIONS; SHIFTS; H2O; AIR
AB Reliable infrared (IR) line lists are reported for the 13 isotopologues of carbon dioxide in HITRAN notation: 626, 636, 628, 627, 828, 727, 827, 638, 637, 737, 838, 738, and 646. Three IR lists are available for each istotopologue: a complete list at 296 K, a reduced-size list at 296 K, plus a reduced-size list at 1000 K. They are denoted Ames-296K, Ames-296K. reduced and Ames-1000K.reduced. With J up to 150, and energy up to 18,000 cm(-1) above the zero point energy, these lists are expected to cover the temperature range up to 1500 K. Line shape parameters including temperature dependence are calculated and reported for four temperature ranges: Mars, Earth, Venus, and Hotter (700-2000 K). Comparisons are made against the available transition data in the HITRAN2012 models. Line position accuracy for most transitions up to 10,000-13,000 cm(-1) is better than 0.03-0.05 cm(-1). Computed transition intensities agree well with most HITRAN data but there exist suspicious exceptions for isotopologues. These line lists will expedite CO2 IR experimental data analysis and provide the scientific community with trustworthy alternatives for unknown IR bands. These line lists may be combined with existing experimental databases to facilitate the analysis of future laboratory experiments or astronomical observations. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Huang, Xinchuan; Freedman, Richard S.] SETI Inst, Mountain View, CA 94043 USA.
   [Gamache, Robert R.] Univ Massachusetts Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA.
   [Schwenke, David W.] NASA, Ames Res Ctr, NAS Facil, MS T27B 1, Moffett Field, CA 94035 USA.
   [Lee, Timothy J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245 1, Moffett Field, CA 94035 USA.
RP Huang, XC (reprint author), SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA.
EM Xinchuan.Huang-1@nasa.gov; Robert_Gamache@uml.edu;
   Richard.S.Freedman@nasa.gov; David.W.Schwenke@nasa.gov;
   Timothy.J.Lee@nasa.gov
RI Lee, Timothy/K-2838-2012; schwenke, david/I-3564-2013; HUANG,
   XINCHUAN/A-3266-2013
FU NASA Venus Express Supporting Investigator Program; NASA/SETI
   [NNX12AG96A, NNX12AJ19A]; National Science Foundation [AGS-1156862];
   NASA ROSES [NNH11ZDA-001N11-OSS-0134, NNH11ZDA001N11-PATM11-0014]
FX DWS, TJL, and XH gratefully acknowledge financial support from the NASA
   Venus Express Supporting Investigator Program. Huang acknowledges the
   NASA/SETI Co-operative Agreement NNX12AG96A. RRG is pleased to
   acknowledge support of this research by the National Science Foundation
   through Grant no. AGS-1156862. R.S. Freedman acknowledges the NASA/SETI
   Co-operative Agreement NNX12AJ19A and NASA ROSES funding
   NNH11ZDA-001N11-OSS-0134 and NNH11ZDA001N11-PATM11-0014. We sincerely
   thank Dr. Sergey Tashkun (V.E. Zuev Institute of Atmospheric Optics,
   Russian Academy of Sciences) for useful discussions and suggestions.
NR 18
TC 24
Z9 25
U1 2
U2 14
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD NOV
PY 2014
VL 147
BP 134
EP 144
DI 10.1016/j.jqsrt.2014.05.015
PG 11
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AN6GY
UT WOS:000340694200015
ER

PT J
AU Gunapala, SD
   Bandara, SV
   Liu, JK
   Mumolo, JM
   Rafol, SB
   Ting, DZ
   Soibel, A
   Hill, C
AF Gunapala, Sarath D.
   Bandara, Sumith V.
   Liu, John K.
   Mumolo, Jason M.
   Rafol, Sir B.
   Ting, David Z.
   Soibel, Alexander
   Hill, Cory
TI Quantum Well Infrared Photodetector Technology and Applications
SO IEEE JOURNAL OF SELECTED TOPICS IN QUANTUM ELECTRONICS
LA English
DT Article
DE Infrared detectors; focal plane arrays; infrared imaging; quantum well
   devices
ID FOCAL-PLANE ARRAYS; INTERSUBBAND ABSORPTION; GRATING COUPLER;
   NARROW-BAND; BROAD-BAND; WAVE-GUIDE; PERFORMANCE; DETECTORS; EFFICIENCY
AB Quantum well infrared photodetectors (QWIPs) are known for their stability, high pixel-to-pixel uniformity, and high-pixel operability, which are essential for large area imaging arrays. In this paper, we discuss the initial demonstration of QWIP devices, and the many years of progress that propelled this technology toward the demonstration of large format focal plane arrays. In addition, we present some potential applications of this technology in science and medicine.
C1 [Gunapala, Sarath D.; Bandara, Sumith V.; Liu, John K.; Mumolo, Jason M.; Rafol, Sir B.; Ting, David Z.; Soibel, Alexander; Hill, Cory] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gunapala, SD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM sarath.d.gunapala@jpl.nasa.gov; sumith.v.bandara.civ@mail.mil;
   John.k.liu@jpl.nasa.gov; jason.m.mumolo@jpl.nasa.gov;
   sir.b.rafol@jpl.nasa.gov; david.z.ting@jpl.nasa.gov;
   alexander.soibel@jpl.nasa.gov; cory.j.hill@jpl.nasa.gov
RI Soibel, Alexander/A-1313-2007
FU Jet Propulsion Laboratory, California Institute of Technology; National
   Aeronautics and Space Administration; Missile Defense Agency; Air Force
   Research Laboratory
FX This work was supported by the Jet Propulsion Laboratory, California
   Institute of Technology, under a contract with the National Aeronautics
   and Space Administration, and was sponsored by the Missile Defense
   Agency and the Air Force Research Laboratory.
NR 32
TC 3
Z9 3
U1 2
U2 51
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1077-260X
EI 1558-4542
J9 IEEE J SEL TOP QUANT
JI IEEE J. Sel. Top. Quantum Electron.
PD NOV-DEC
PY 2014
VL 20
IS 6
AR 3802312
DI 10.1109/JSTQE.2014.2324538
PG 12
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA AN3ZK
UT WOS:000340527200001
ER

PT J
AU Thompson, DR
   Green, RO
   Keymeulen, D
   Lundeen, SK
   Mouradi, Y
   Nunes, DC
   Castano, R
   Chien, SA
AF Thompson, David R.
   Green, Robert O.
   Keymeulen, Didier
   Lundeen, Sarah K.
   Mouradi, Yasha
   Nunes, Daniel Cahn
   Castano, Rebecca
   Chien, Steve A.
TI Rapid Spectral Cloud Screening Onboard Aircraft and Spacecraft
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Cloud screening; imaging spectroscopy; lossy compression; pattern
   recognition; real-time systems
ID IMAGING SPECTROMETER AVIRIS; MODIS; COVER; SNOW; CLASSIFICATION;
   SPECTROSCOPY; VALIDATION; RETRIEVAL; ALGORITHM; MISSION
AB Next-generation orbital imaging spectrometers will generate unprecedented data volumes, demanding new methods to optimize storage and communication resources. Here, we demonstrate that onboard analysis can excise cloud-contaminated scenes, reducing data volumes while preserving science return. We calculate optimal cloud-screening parameters in advance, exploiting stable radiometric calibration and foreknowledge of illumination and viewing geometry. Channel thresholds expressed in raw instrument values can be then uploaded to the sensor where they execute in real time at gigabit-per-second (Gb/s) data rates. We present a decision theoretic method for setting these instrument parameters and characterize performance using a continuous three-year image archive from the "classic" Airborne Visible/Infrared Imaging Spectrometer (AVIRIS-C). We then simulate the system onboard the International Space Station, where it provides factor-of-two improvements in data volume with negligible false positives. Finally, we describe a real-time demonstration onboard the AVIRIS Next Generation (AVIRIS-NG) flight platform during a recent science campaign. In this blind test, cloud screening is performed without error while keeping pace with instrument data rates.
C1 [Thompson, David R.; Green, Robert O.; Keymeulen, Didier; Lundeen, Sarah K.; Mouradi, Yasha; Nunes, Daniel Cahn; Castano, Rebecca; Chien, Steve A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Thompson, DR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU National Aeronautics and Space Administration
FX The Airborne Visible/Infrared Imaging Spectrometer is operated by JPL
   with support from the National Aeronautics and Space Administration. The
   MODIS land-cover data were obtained through the online Data Pool at the
   NASA Land Processes Distributed Active Archive Center (LP DAAC),
   USGS/Earth Resources Observation and Science (EROS) Center, Sioux Falls,
   SD.
NR 47
TC 6
Z9 7
U1 1
U2 24
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 NOV
PY 2014
VL 52
IS 11
BP 6779
EP 6792
DI 10.1109/TGRS.2014.2302587
PG 14
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
   Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
   & Photographic Technology
GA AN0MN
UT WOS:000340278800001
ER

PT J
AU Podest, E
   McDonald, KC
   Kimball, JS
AF Podest, Erika
   McDonald, Kyle C.
   Kimball, John S.
TI Multisensor Microwave Sensitivity to Freeze/Thaw Dynamics Across a
   Complex Boreal Landscape
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Freeze; radar; remote sensing; thaw
ID LAND-SURFACE TEMPERATURE; NASA SCATTEROMETER NSCAT; IMAGING RADAR;
   CARBON BALANCE; SOIL-MOISTURE; SPRING THAW; ERS-1 SAR; SEASONS; STATE;
   VEGETATION
AB The annual freeze/thaw (FT) cycle determines the potential growing season in boreal landscapes and is a major factor determining ecosystem productivity and associated exchange of trace gases (CO2, H2O) with the atmosphere. Accurate characterization of these processes can improve regional assessment of seasonal carbon dynamics and climate feedbacks. FT process variations are spatially and temporally complex due to topography, snow depth and wetness, land cover, or local climatic conditions. In this paper, we perform a landscape analysis of multifrequency and multitemporal satellite microwave remote sensing measurements at L-band (JERS-1), C-band (ERS), and Ku-band (QuikSCAT) for characterizing FT dynamics. We first analyze backscatter sensitivity of the three frequencies to FT conditions over selected Alaska temperature sites. We then apply an FT classifier over two study areas (wetland complex and moderate topography) and examine differences in FT timing according to vegetation, elevation, and north/south facing slope. Results show that L-, C-, and Ku-band backscatter are sensitive to landscape FT state transitions, with higher backscatter for nonfrozen than frozen conditions at C- and L-bands but the opposite response at Ku-band. We applied a change detection algorithm to the C-band and L-band data over both study areas and analyzed the FT classifications with land cover information. These results resolve characteristic patterns of earlier spring thawing for south facing slopes, lower elevations, and coniferous vegetation. Our results also inform similar FT algorithm development for the NASA Soil Moisture Active Passive mission by documenting L-band FT sensitivity and heterogeneity over a boreal landscape.
C1 [Podest, Erika; McDonald, Kyle C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [McDonald, Kyle C.] CUNY, City Coll New York, New York, NY 10031 USA.
   [Kimball, John S.] Univ Montana, Flathead Lake Biol Stn, Div Biol Sci, Polson, MT 59812 USA.
   [Kimball, John S.] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA.
RP Podest, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kmcdonald2@ccny.cuny.edu; johnk@flbs.umt.edu
FU NASA
FX This work was supported by grants from NASA's Advanced Development
   Research Opportunity, Terrestrial Ecology, Terrestrial Hydrology, and
   Making Earth System Data Records for Use in Research Environments
   (MEaSUREs) programs and was undertaken in part within the framework of
   the JAXA Kyoto & Carbon Initiative.
NR 57
TC 7
Z9 7
U1 3
U2 54
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 NOV
PY 2014
VL 52
IS 11
BP 6818
EP 6828
DI 10.1109/TGRS.2014.2303635
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 AN0MN
UT WOS:000340278800004
ER

PT J
AU Sy, OO
   Tanelli, S
   Kollias, P
   Ohno, Y
AF Sy, Ousmane O.
   Tanelli, Simone
   Kollias, Pavlos
   Ohno, Yuichi
TI Application of Matched Statistical Filters for EarthCARE Cloud Doppler
   Products
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Entropy; matched filters; pulse Doppler radar; random noise; spaceborne
   radar
ID PROFILING RADAR; VELOCITY-MEASUREMENTS; RAINFALL
AB This paper presents a method for filtering the random noise that affects spaceborne Doppler measurements of atmospheric velocities. The proposed method hinges on adaptive low-pass filters that apply to the measured pulse-pair correlation function. The parameters of the filters are found by optimizing the statistics of the velocity residue of the filter. The method is illustrated by simulations of the cloud-profiling radar of the future Earth Cloud, Aerosol and Radiation Explorer (EarthCARE) mission of the European Space Agency and the Japanese Space Exploration Agency. These simulations, which do not include strong convection, show the higher performance of the filters when compared with the traditional increase of the along-track integration length. The results obtained with the filters show that velocity accuracies of 0.48, 0.42, and 0.39 m . s(-1) are achievable at PRF = {6.1, 7, 7.5} kHz, respectively, while preserving the initial 500-m sampling of the measured EarthCARE data. These results also show the potential benefits of avoiding excessive along-track integration, for postprocessing tasks such as dealiasing or the retrieval of the vertical distribution of the atmospheric velocity (e. g., longer than 5 km for cases consistent with the climatologies represented in this data set).
C1 [Sy, Ousmane O.; Tanelli, Simone] CALTECH, Jet Prop Lab, Radar Sci & Engn Dept, Pasadena, CA 91109 USA.
   [Kollias, Pavlos] McGill Univ, Montreal, PQ H3A 0G4, Canada.
   [Ohno, Yuichi] Natl Inst Informat & Commun Technol, Koganei, Tokyo 1848795, Japan.
RP Sy, OO (reprint author), CALTECH, Jet Prop Lab, Radar Sci & Engn Dept, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ousmane.o.sy@jpl.nasa.gov; simone.tanelli@jpl.nasa.gov;
   pavlos.kollias@mcgill.ca; ohno@nict.go.jp
FU NASA Stand Alone Mission of Opportunity Notice/U.S. Participating
   Investigator program
FX The research described in this paper was carried out at the Jet
   Propulsion Laboratory, California Institute of Technology, under a
   contract with the National Aeronautics and Space Administration. The
   authors would like to thank the NASA Stand Alone Mission of Opportunity
   Notice/U.S. Participating Investigator program for the support. They
   would also like to thank the reviewers for their constructive remarks.
NR 21
TC 4
Z9 4
U1 0
U2 8
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 NOV
PY 2014
VL 52
IS 11
BP 7297
EP 7316
DI 10.1109/TGRS.2014.2311031
PG 20
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
   Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
   & Photographic Technology
GA AN0MN
UT WOS:000340278800043
ER

PT J
AU Brucker, L
   Cavalieri, DJ
   Markus, T
   Ivanoff, A
AF Brucker, Ludovic
   Cavalieri, Donald J.
   Markus, Thorsten
   Ivanoff, Alvaro
TI NASA Team 2 Sea Ice Concentration Algorithm Retrieval Uncertainty
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Measurement uncertainty; passive microwave remote sensing; sea ice
ID AMSR-E; VALIDATION; IMAGERY; MODIS; EOS
AB Satellite microwave radiometers are widely used to estimate sea ice cover properties (concentration, extent, and area) through the use of sea ice concentration (IC) algorithms. Rare are the algorithms providing associated IC uncertainty estimates. Algorithm uncertainty estimates are needed to assess accurately global and regional trends in IC (and thus extent and area), and to improve sea ice predictions on seasonal to interannual timescales using data assimilation approaches. This paper presents a method to provide relative IC uncertainty estimates using the enhanced NASA Team (NT2) IC algorithm. The proposed approach takes advantage of the NT2 calculations and solely relies on the brightness temperatures (TBs) used as input. NT2 IC and its associated relative uncertainty are obtained for both the Northern and Southern Hemispheres using the Advanced Microwave Scanning Radiometer for the Earth Observing System (AMSR-E) TB. NT2 IC relative uncertainties estimated on a footprint-by-footprint swath-by-swath basis were averaged daily over each 12.5-km grid cell of the polar stereographic grid. For both hemispheres and throughout the year, the NT2 relative uncertainty is <5%. In the Southern Hemisphere, it is low in the interior ice pack, and it increases in the marginal ice zone up to 5%. In the Northern Hemisphere, areas with high uncertainties are also found in the high IC area of the Central Arctic. Retrieval uncertainties are greater in areas corresponding to NT2 ice types associated with deep snow and new ice. Seasonal variations in uncertainty show larger values in summer as a result of melt conditions and greater atmospheric contributions. Our analysis also includes an evaluation of the NT2 algorithm sensitivity to AMSR-E sensor noise. There is a 60% probability that the IC does not change (to within the computed retrieval precision of 1%) due to sensor noise, and the cumulated probability shows that there is a 90% chance that the IC varies by less than +/- 3%. We also examined the daily IC variability, which is dominated by sea ice drift and ice formation/melt. Daily IC variability is the highest, year round, in the MIZ (often up to 20%, locally 30%). The temporal and spatial distributions of the retrieval uncertainties and the daily IC variability is expected to be useful for algorithm intercomparisons, climate trend assessments, and possibly IC assimilation in models.
C1 [Brucker, Ludovic; Cavalieri, Donald J.; Markus, Thorsten; Ivanoff, Alvaro] 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.
   [Cavalieri, Donald J.] DJ Cavalieri, Sandy Spring, MD 20860 USA.
   [Ivanoff, Alvaro] ADNET Syst Inc, Rockville, MD 20852 USA.
RP Brucker, L (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
EM ludovic.brucker@nasa.gov; Donald.J.Cavalieri@nasa.gov;
   thorsten.markus@nasa.gov; alvaro.ivanoff@nasa.gov
RI Brucker, Ludovic/A-8029-2010
OI Brucker, Ludovic/0000-0001-7102-8084
NR 24
TC 5
Z9 5
U1 2
U2 34
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 NOV
PY 2014
VL 52
IS 11
BP 7336
EP 7352
DI 10.1109/TGRS.2014.2311376
PG 17
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
   Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
   & Photographic Technology
GA AN0MN
UT WOS:000340278800046
ER

PT J
AU Wang, PJ
   Gao, F
   Masek, JG
AF Wang, Peijuan
   Gao, Feng
   Masek, Jeffrey G.
TI Operational Data Fusion Framework for Building Frequent Landsat-Like
   Imagery
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Crop condition monitoring; data fusion; Landsat; Moderate Resolution
   Imaging Spectroradiometer (MODIS); spatial and temporal adaptive
   reflectance fusion model (STARFM); time series; vegetation index (VI)
ID MODIS DATA; REFLECTANCE; GENERATION; PRODUCTS; ALBEDO; MODEL; BRDF
AB An operational data fusion framework was built to generate dense time-series Landsat-like images by fusing MODIS data products and Landsat imagery. The spatial and temporal adaptive reflectance fusion model (STARFM) was integrated in the framework. Compared with earlier implementations of the STARFM, several improvements have been incorporated in the operational data fusion framework. These include viewing angular correction on the MODIS daily bidirectional reflectance, precise and automated coregistration on MODIS and Landsat paired images, and automatic selection of Landsat and MODIS paired dates. Three tests that use MODIS and Landsat data pairs from the same season of the same year, the same season of two different years, and different seasons from adjacent years were performed over a Landsat scene in northern India using the integrated STARFM operational framework. The results show that the accuracy of the predicted results depends on the data consistency between the MODIS nadir bidirectional-reflectance-distribution-function-adjusted reflectance and Landsat surface reflectance on both the paired dates and the prediction dates. When MODIS and Landsat reflectances were consistent, the maximum difference of the predicted results for all Landsat spectral bands, except the blue band, was about 0.007 (or 5.1% relatively). However, differences were larger (0.026 in absolute and 13.8% in relative, except the blue band) when two data sources were inconsistent. In an extreme case, the difference for blue-band reflectance was as large as 0.029 (or 39.1% relatively). Case studies focused on monitoring vegetation condition in central India and the Hindu Kush Himalayan region. In general, spatial and temporal landscape variation could be identified with a high level of detail from the fused data. Vegetation index trajectories derived from the fused products could be associated with specific land cover types that occur in the study regions. The operational data fusion framework provides a feasible and cost-effective way to build dense time-series images at Landsat spatial resolution for cloudy regions.
C1 [Wang, Peijuan] Chinese Acad Meteorol Sci, Beijing 100081, Peoples R China.
   [Wang, Peijuan; Gao, Feng] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA.
   [Masek, Jeffrey G.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
RP Wang, PJ (reprint author), Chinese Acad Meteorol Sci, Beijing 100081, Peoples R China.
EM wangpj@cams.cma.gov.cn; Feng.Gao@ars.usda.gov; jeffrey.g.masek@nasa.gov
RI Masek, Jeffrey/D-7673-2012
FU NASA Research Program; Landsat Science Team Project; National Basic
   Research Program of China [2010CB951304]; National Natural Science
   Foundation of China [41371410, 41071224]; Basic Research and Operating
   Expenses of CAMS [2013Y006]
FX This work was supported in part by the NASA Research Program, by the
   Landsat Science Team Project, by the National Basic Research Program of
   China under Grant 2010CB951304, by the National Natural Science
   Foundation of China under Grant 41371410 and Grant 41071224, and by the
   Basic Research and Operating Expenses of CAMS under Grant 2013Y006.
NR 23
TC 8
Z9 8
U1 3
U2 18
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 NOV
PY 2014
VL 52
IS 11
BP 7353
EP 7365
DI 10.1109/TGRS.2014.2311445
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 AN0MN
UT WOS:000340278800047
ER

PT J
AU Brucker, L
   Dinnat, EP
   Picard, G
   Champollion, N
AF Brucker, Ludovic
   Dinnat, Emmanuel P.
   Picard, Ghislain
   Champollion, Nicolas
TI Effect of Snow Surface Metamorphism on Aquarius L-Band Radiometer
   Observations at Dome C, Antarctica
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aquarius; cryosphere; L-band; microwave radiometry
ID MICROWAVE BRIGHTNESS TEMPERATURE; MODELING TIME-SERIES; MASS-BALANCE;
   ICE-SHEET; PLATEAU; EMISSION; ACCUMULATION; VARIABILITY; SATELLITE;
   FIELD
AB The Antarctic Plateau presents ideal characteristics to study the relationship between microwave observations and snow/ice properties. It is also a promising target for radiometer calibration and sensor intercalibration, which are critical for applications requiring subkelvin accuracy, such as sea surface salinity retrievals. This paper presents the spaceborne Aquarius L-band radiometric observations collected since August 2011 over the Antarctic Plateau, and it focuses on their temporal evolutions at Dome C (75.1 degrees S, 123.35 degrees E). Aquarius operates three radiometers with a sensitivity of 0.15 K (over the oceans), allowing us to analyze small variations in brightness temperature (TB) and changes with incidence angles. Over the Antarctic Plateau, Aquarius TBs have a relatively low annual standard deviation (0.2-0.9 K) where melting never occurs. However, the analysis of the TB time series at Dome C revealed significant variations (up to 2.5 K) in summer. First, these variations are compared with a remote sensing grain index (GI) based on high-frequency (89 and 150 GHz) shallow-penetration TB channels. Variations in the ratio of TBs observed at horizontal and vertical polarizations are synchronous with GI changes. Second, Aquarius TB variations are compared with the presence of hoar crystals on the surface identified using surface-based near-infrared photographs. The largest and longest changes in TBs correspond to periods with hoar crystals on the surface. Therefore, in spite of the deep penetration of the L-band radiation, evolutions of the snow properties near the surface, which usually change rapidly and irregularly, do influence L-band observations. Collection of accurate snow surface measurements and thorough analyses of the L-band observations are thus needed to use the Antarctic Plateau as a calibration/inter-calibration target.
C1 [Brucker, Ludovic; Dinnat, Emmanuel P.] 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.
   [Dinnat, Emmanuel P.] Chapman Univ, Sch Earth & Environm Sci, Orange, CA 92866 USA.
   [Picard, Ghislain; Champollion, Nicolas] Univ Grenoble Alpes, CNRS, Lab Glaciol & Geophys Environm, F-38041 Grenoble, France.
RP Brucker, L (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
EM ludovic.brucker@nasa.gov; emmanuel.dinnat@nasa.gov;
   ghislain.picard@lgge.obs.ujf-grenoble.fr;
   nicolas.champollion@lgge.obs.ujf-grenoble.fr
RI Dinnat, Emmanuel/D-7064-2012; Champollion, Nicolas/B-7921-2014; Brucker,
   Ludovic/A-8029-2010; Picard, Ghislain/D-4246-2013
OI Dinnat, Emmanuel/0000-0001-9003-1182; Champollion,
   Nicolas/0000-0001-7988-4694; Brucker, Ludovic/0000-0001-7102-8084;
   Picard, Ghislain/0000-0003-1475-5853
NR 44
TC 14
Z9 14
U1 2
U2 30
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 NOV
PY 2014
VL 52
IS 11
BP 7408
EP 7417
DI 10.1109/TGRS.2014.2312102
PG 10
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
   Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
   & Photographic Technology
GA AN0MN
UT WOS:000340278800051
ER

PT J
AU Stiles, BW
   Danielson, RE
   Poulsen, WL
   Brennan, MJ
   Hristova-Veleva, S
   Shen, TP
   Fore, AG
AF Stiles, Bryan W.
   Danielson, Richard E.
   Poulsen, W. Lee
   Brennan, Michael J.
   Hristova-Veleva, Svetla
   Shen, Tsae-Pyng
   Fore, Alexander G.
TI Optimized Tropical Cyclone Winds From QuikSCAT: A Neural Network
   Approach
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Radar remote sensing; spaceborne radar; tropical cyclones
ID NATIONAL HURRICANE CENTER; VECTOR RETRIEVAL; RAIN RETRIEVAL; SURFACE
   WINDS; SCATTEROMETER; IMPACT; MODEL; SIMULATIONS; CHALLENGES; PREDICTION
AB We have developed a neural network technique for retrieving accurate 12.5-km resolution wind speeds from Ku-band scatterometer measurements in tropical cyclone conditions including typical rain events in such storms. The method was shown to retrieve accurate wind speeds up to 40 m/s when compared with aircraft reconnaissance data, including GPS dropwindsondes and Stepped-Frequency Microwave Radiometer surface wind speed measurements, and when compared to global best track maximum wind speeds. Wind directions were unchanged from the current (version 3) Jet Propulsion Laboratory (JPL) global wind vector product. The technique removes positive biases with respect to best track winds in the developing phase of tropical cyclones that occurred in the nominal (version 2) JPL QuikSCAT product. The new technique also reduces negative biases with respect to best track wind speeds that occurred in the nominal product (both versions 2 and 3) during the most extreme period of the lifetime of intense storms. The wind regime with the most notable improvement is 20-40 m/s (40-80 kn), with more modest improvement for higher winds and the improvement at lower winds comparable to that achieved previously by the version 3 JPL global rain-corrected product. The net effect of all the wind speed improvements is a much better measurement of storm intensity over time in the new product than what has been previously available. When compared with speed data from aircraft flights in Atlantic hurricanes, the new product exhibited a 1-2-m/s positive overall bias and a 3-m/s mean absolute error. The random error and systematic positive bias in the new scatterometer wind product is similar to that of the Hurricane Research Division H*WIND analyses when aircraft data are available for assimilation. This similarity may be explained by the fact that H*WIND data are used as ground truth to fit the coefficients used by the new technique to map radar measurements to wind speed. The fact that H*WIND was designed to match maximum winds while preserving radial symmetry may explain the overall positive biases that we observe in both H*WIND and the new scatterometer wind product which compared to aircraft reconnaissance data. The new scatterometer product could also be inheriting systematic biases in the presence of rain from H*WIND. Under the most extreme rain conditions, the radar signal from the surface can be lost. In such cases, the technique makes use of measurements in the 87.5-km region comprising the 7 x 7 neighboring cells around the target 12.5-km wind vector cell. In so doing, we sacrifice resolution in cases where the highest resolution region has no useful measurements. Even so, the most extreme rain conditions can result in reduced accuracy. The new technique has been used to retrieve wind fields for every tropical cyclone of tropical storm force or above that has been observed by QuikSCAT during the period of time from October 1999 to November 2009. The resulting data set has been made available online for use by the tropical cyclone research community.
C1 [Stiles, Bryan W.; Poulsen, W. Lee; Hristova-Veleva, Svetla; Shen, Tsae-Pyng; Fore, Alexander G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Danielson, Richard E.; Brennan, Michael J.] NOAA, Natl Weather Serv, Natl Ctr Environm Predict, Natl Hurricane Ctr, Miami, FL 33165 USA.
RP Stiles, BW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 51
TC 7
Z9 7
U1 0
U2 19
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 NOV
PY 2014
VL 52
IS 11
BP 7418
EP 7434
DI 10.1109/TGRS.2014.2312333
PG 17
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
   Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
   & Photographic Technology
GA AN0MN
UT WOS:000340278800052
ER

PT J
AU Salem, JA
   Quinn, GD
AF Salem, Jonathan A.
   Quinn, George D.
TI Fractographic analysis of large single crystal sapphire refractive
   secondary concentrators
SO JOURNAL OF THE EUROPEAN CERAMIC SOCIETY
LA English
DT Article; Proceedings Paper
CT Fractography of advanced ceramics IV
CY SEP 29-OCT 02, 2013
CL Smolenice, SLOVAKIA
DE Failure analysis; Fractography; Sapphire; Solar concentrator; Twins;
   Polishing flaws; Finite element analysis; Thermal stresses; Solar
   energy; Space exploration; Strength
ID STRENGTH
AB A fractographic analysis was performed on two large (9.5 cm diameter x 28 cm long) sapphire single crystal refractive concentrators that broke during elevated temperature testing in a space simulation chamber. Both concentrators failed from machining/handling damage on the lens face. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Salem, Jonathan A.] NASA, Glenn Res Ctr, Cleveland, OH USA.
   [Quinn, George D.] NIST, Gaithersburg, MD 20899 USA.
RP Quinn, GD (reprint author), NIST, Gaithersburg, MD 20899 USA.
EM george.quinn@nist.gov
NR 13
TC 0
Z9 0
U1 1
U2 7
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 NOV
PY 2014
VL 34
IS 14
SI SI
BP 3271
EP 3281
DI 10.1016/j.jeurceramsoc.2014.01.029
PG 11
WC Materials Science, Ceramics
SC Materials Science
GA AM9TB
UT WOS:000340222800005
ER

PT J
AU Coyle, DB
   Stysley, PR
   Poulios, D
   Fredrickson, RM
   Kay, RB
   Cory, KC
AF Coyle, D. Barry
   Stysley, Paul R.
   Poulios, Demetrios
   Fredrickson, Robert M.
   Kay, Richard B.
   Cory, Kenneth C.
TI High efficiency, 100 mJ per pulse, Nd:YAG oscillator optimized for
   space-based earth and planetary remote sensing
SO OPTICS AND LASER TECHNOLOGY
LA English
DT Article
DE Laser; Nd:YAG; Q-switched
ID LASER
AB We report on a newly solid state laser transmitter, designed and packaged for Earth and planetary space-based remote sensing applications for high efficiency, low part count, high pulse energy scalability/stability, and long life. Finally, we have completed a long term operational test which surpassed 2 Billion pulses with no measured decay in pulse energy. Published by Elsevier Ltd.
C1 [Coyle, D. Barry; Stysley, Paul R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Poulios, Demetrios; Kay, Richard B.] Amer Univ, Dept Phys, Washington, DC 20016 USA.
   [Fredrickson, Robert M.; Cory, Kenneth C.] Sigma Space Corp, Lanham, MD 20706 USA.
RP Coyle, DB (reprint author), NASA, Goddard Space Flight Ctr, Code 554, Greenbelt, MD 20771 USA.
EM barry.coyle@nasa.gov
NR 8
TC 4
Z9 4
U1 2
U2 22
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0030-3992
EI 1879-2545
J9 OPT LASER TECHNOL
JI Opt. Laser Technol.
PD NOV
PY 2014
VL 63
BP 13
EP 18
DI 10.1016/j.optlastec.2014.03.009
PG 6
WC Optics; Physics, Applied
SC Optics; Physics
GA AJ7KV
UT WOS:000337876500003
ER

PT J
AU Zamparelli, V
   Agram, PS
   Fornaro, G
AF Zamparelli, V.
   Agram, P. S.
   Fornaro, G.
TI Estimation and Compensation of Phase Shifts in SAR Focusing of Spotlight
   Data Acquired With Discrete Antenna Steering
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Image contrast method; spotlight mode; synthetic aperture radar (SAR)
   focusing
ID TERRASAR-X
AB Modern spaceborne synthetic aperture radar sensors are able to operate the spotlight mode to achieve very high resolution images at microwave frequencies. This mode is characterized by antenna steering to increase the illumination interval. The steering is carried out by beam switching on bursts during the data acquisition interval. In addition to an unavoidable spectrum modulation in azimuth, phase shifts can occur from burst to burst. In this letter, we describe the problem and a procedure able to estimate the phase shifts based on the image contrast maximization technique for subsequent compensation at the data focusing stage. Results on real data acquired by the COSMO-SkyMed sensor demonstrate the effectiveness of the proposed solution.
C1 [Zamparelli, V.; Fornaro, G.] CNR, Inst Elect Sensing Environm IREA, Natl Res Council, I-80124 Naples, Italy.
   [Agram, P. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Zamparelli, V (reprint author), CNR, Inst Elect Sensing Environm IREA, Natl Res Council, I-80124 Naples, Italy.
EM zamparelli.v@irea.cnr.it; piyush.agram@jpl.nasa.gov;
   fornaro.g@irea.cnr.it
OI Fornaro, Gianfranco/0000-0002-1679-607X
NR 13
TC 1
Z9 1
U1 0
U2 12
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 NOV
PY 2014
VL 11
IS 11
BP 1921
EP 1925
DI 10.1109/LGRS.2014.2313914
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 AI9SV
UT WOS:000337277500014
ER

PT J
AU Kogan, O
   Khasin, M
   Meerson, B
   Schneider, D
   Myers, CR
AF Kogan, Oleg
   Khasin, Michael
   Meerson, Baruch
   Schneider, David
   Myers, Christopher R.
TI Two-strain competition in quasineutral stochastic disease dynamics
SO PHYSICAL REVIEW E
LA English
DT Article
ID STATIONARY DISTRIBUTION; DENSITY-DEPENDENCE; LOGISTIC MODEL; EXTINCTION;
   POPULATIONS; EPIDEMICS; OUTBREAKS; FIXATION; TIMES
AB We develop a perturbation method for studying quasineutral competition in a broad class of stochastic competition models and apply it to the analysis of fixation of competing strains in two epidemic models. The first model is a two-strain generalization of the stochastic susceptible-infected-susceptible (SIS) model. Here we extend previous results due to Parsons and Quince [Theor. Popul. Biol. 72, 468 (2007)], Parsons et al. [Theor. Popul. Biol. 74, 302 (2008)], and Lin, Kim, and Doering [J. Stat. Phys. 148, 646 (2012)]. The second model, a two-strain generalization of the stochastic susceptible-infected-recovered (SIR) model with population turnover, has not been studied previously. In each of the two models, when the basic reproduction numbers of the two strains are identical, a system with an infinite population size approaches a point on the deterministic coexistence line (CL): a straight line of fixed points in the phase space of subpopulation sizes. Shot noise drives one of the strain populations to fixation, and the other to extinction, on a time scale proportional to the total population size. Our perturbation method explicitly tracks the dynamics of the probability distribution of the subpopulations in the vicinity of the CL. We argue that, whereas the slow strain has a competitive advantage for mathematically "typical" initial conditions, it is the fast strain that is more likely to win in the important situation when a few infectives of both strains are introduced into a susceptible population.
C1 [Kogan, Oleg; Myers, Christopher R.] Cornell Univ, Lab Atom & Solid State Phys, Ithaca, NY 14853 USA.
   [Khasin, Michael] SGT Inc, NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
   [Meerson, Baruch] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
   [Schneider, David] ARS, Robert W Holley Ctr Agr & Hlth, USDA, Ithaca, NY 14853 USA.
   [Schneider, David] Cornell Univ, Dept Plant Pathol & Plant Microbe Biol, Ithaca, NY 14853 USA.
   [Myers, Christopher R.] Cornell Univ, Inst Biotechnol, Ithaca, NY 14853 USA.
RP Kogan, O (reprint author), Cornell Univ, Lab Atom & Solid State Phys, Ithaca, NY 14853 USA.
EM obk5@cornell.edu
RI Schneider, David/H-2236-2012
OI Schneider, David/0000-0002-2124-8385
FU United States-Israel Binational Science Foundation (BSF) [2012145];
   Science & Technology Directorate, Department of Homeland Security
   [HSHQDC-10-X-00138]
FX We are grateful to Charles R. Doering and Leonard M. Sander for
   attracting our interest in quasineutral competition and to Michael C.
   Cross and Mark I. Dykman for a discussion of phase diffusion and drift
   in noisy limit cycles. This research was supported in part by Grant No.
   2012145 from the United States-Israel Binational Science Foundation
   (BSF), and in part by the Science & Technology Directorate, Department
   of Homeland Security via interagency Agreement No. HSHQDC-10-X-00138.
   B.M. acknowledges the hospitality of the Michigan Center for Theoretical
   Physics, where this project was started.
NR 44
TC 8
Z9 8
U1 0
U2 4
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0045
EI 2470-0053
J9 PHYS REV E
JI Phys. Rev. E
PD OCT 31
PY 2014
VL 90
IS 4
AR 042149
DI 10.1103/PhysRevE.90.042149
PG 17
WC Physics, Fluids & Plasmas; Physics, Mathematical
SC Physics
GA AS2HO
UT WOS:000344100800004
PM 25375480
ER

PT J
AU Huang, J
   Feng, LJ
   Lu, DB
   Zhang, QR
   Sun, T
   Chu, XL
AF Huang, Jing
   Feng, Lianjun
   Lu, Dingbiao
   Zhang, Qirui
   Sun, Tao
   Chu, Xuelei
TI Multiple climate cooling prior to Sturtian glaciations: Evidence from
   chemical index of alteration of sediments in South China
SO SCIENTIFIC REPORTS
LA English
DT Article
ID OXYGEN-ISOTOPE SIGNATURE; CONTINENTAL BREAK-UP; NEOPROTEROZOIC
   GLACIATIONS; SNOWBALL EARTH; YANGTZE PLATFORM; AGE CONSTRAINTS; METEORIC
   WATER; NANHUA SYSTEM; COLD CLIMATE; ZIRCON
AB Investigation of climatic conditions prior to the Sturtian glaciations is critical to understanding the trigger mechanism for the series of Neoproterozoic global glaciations. In this study, we report high-resolution chemical index of alteration (CIA) records in the sediments of South China prior to the Sturtian glaciation (820,720 Ma). Our results showed there occurred multiple climate cooling before the Sturtian glaciations in South China: (1) a series of episodic and possibly global climate cooling periods from ca. 750 Ma to 725 Ma, which also caused some diachronous regional glaciations; (2) a permanent climate cooling period between ca. 800 Ma and 770 Ma, probably contemporaneous to the global "Bitter Springs stage'' delta C-13 negative excursion; (3) a climate cooling period between ca. 815 Ma and 810 Ma. The three stages of climate cooling are also supported by their correspondence to previously reported extremely low delta O-18 records of igneous/metamorphic minerals from South China. These climate cooling periods also coincide with the magmatism and rifting events in South China. We argue that tectonic movements were the primary control on the climate cooling before the Neoproterozoic global glaciations.
C1 [Huang, Jing] Univ Sci & Technol China, Sch Earth & Space Sci, CAS Key Lab Crust Mantle Mat & Environm, Hefei 230026, Peoples R China.
   [Feng, Lianjun; Zhang, Qirui; Chu, Xuelei] Chinese Acad Sci, Inst Geol & Geophys, State Key Lab Lithospher Evolut, Beijing 100029, Peoples R China.
   [Lu, Dingbiao] Guizhou Geol Survey, Guiyang 550002, Peoples R China.
   [Sun, Tao] NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA.
   [Sun, Tao] Louisiana State Univ, Dept Geol & Geophys, Baton Rouge, LA 70803 USA.
   [Chu, Xuelei] Northwest Univ, State Key Lab Continental Dynam, Xian 710069, Peoples R China.
RP Huang, J (reprint author), Univ Sci & Technol China, Sch Earth & Space Sci, CAS Key Lab Crust Mantle Mat & Environm, Hefei 230026, Peoples R China.
EM hjmail@ustc.edu.cn
FU National Basic Research Program of China [2011CB808805, 2013CB835003];
   Natural Science Foundation of China [41373077, 41172029, 41003034,
   41025011]; Fundamental Research Funds for the Central Universities;
   State Key Laboratory of Continental Dynamics, Northwest University in
   China
FX This research is supported by the National Basic Research Program of
   China (Grant 2011CB808805, 2013CB835003), the Natural Science Foundation
   of China (Grants 41373077, 41172029, 41003034, 41025011), the
   Fundamental Research Funds for the Central Universities and the State
   Key Laboratory of Continental Dynamics, Northwest University in China.
   We thank Prof. Huaiwei Ni and Prof. Liping Qin for constructive
   comments. We also thank Prof. Fang Huang, Prof. Yingming Sheng, and
   Prof. Zhenhui Hou for guide in lab.
NR 46
TC 1
Z9 2
U1 4
U2 25
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 OCT 31
PY 2014
VL 4
AR 6868
DI 10.1038/srep06868
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AS0SX
UT WOS:000343989900001
PM 25359610
ER

PT J
AU Peverati, R
   Bera, PP
   Lee, TJ
   Head-Gordon, M
AF Peverati, Roberto
   Bera, Partha P.
   Lee, Timothy J.
   Head-Gordon, Martin
TI Formation and Stability of C6H3+ Isomers
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID DOUBLE AROMATICITY; 3,5-DEHYDROPHENYL CATION; ELECTRON-AFFINITIES;
   TRANSITION-STATES; CARBON RINGS; CLUSTERS; ANTIAROMATICITY;
   THERMOCHEMISTRY; ABSORPTION; ACETYLENE
AB The stability of the five main isomers of C6H3+ was investigated using quantum chemical calculations. The cyclic isomers are stabilized by two complementary aromatic effects, first 6-electron p aromaticity, and second a more unusual three-center two-electron s aromaticity. Two cyclic isomers sit at the bottom of the potential energy surface with energies very close to each other, with a third cyclic isomer slightly higher. The reaction barriers for the interconversion of these isomers, as well as to convert to low-energy linear isomers, are found to be very high with transition states that break both the p and the s aromaticities. Finally, possibilities for forming the cyclic isomers via association reactions are discussed.
C1 [Peverati, Roberto; Head-Gordon, Martin] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
   [Peverati, Roberto; Head-Gordon, Martin] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Chem Sci, Berkeley, CA 94720 USA.
   [Bera, Partha P.; Lee, Timothy J.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
   [Bera, Partha P.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
RP Head-Gordon, M (reprint author), Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.
EM mhg@cchem.berkeley.edu
RI Lee, Timothy/K-2838-2012; Bera, Partha /K-8677-2012; 
OI Peverati, Roberto/0000-0001-7774-9923
FU NASA Carbon in the Galaxy consortium [NNH10ZDA001N]; BAER Institute
FX We acknowledge financial support from the NASA Carbon in the Galaxy
   consortium grant NNH10ZDA001N. PPB also acknowledges support from the
   BAER Institute.
NR 42
TC 3
Z9 3
U1 1
U2 14
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 30
PY 2014
VL 118
IS 43
BP 10109
EP 10116
DI 10.1021/jp5081862
PG 8
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA AS2UU
UT WOS:000344135600020
PM 25285962
ER

PT J
AU Cook, BI
   Seager, R
   Smerdon, JE
AF Cook, Benjamin I.
   Seager, Richard
   Smerdon, Jason E.
TI The worst North American drought year of the last millennium: 1934
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE drought; Dust Bowl; aerosols
ID WESTERN UNITED-STATES; DUST BOWL DROUGHT; LONG-TERM DROUGHT; US
   GREAT-PLAINS; REANALYSIS PROJECT; PRECIPITATION; PREDICTABILITY;
   TEMPERATURE; VARIABILITY; STORMS
AB During the summer of 1934, over 70% of western North America experienced extreme drought, placing this summer far outside the normal range of drought variability and making 1934 the single worst drought year of the last millennium. Strong atmospheric ridging along the West Coast suppressed cold season precipitation across the Northwest, Southwest, and California, a circulation pattern similar to the winters of 1976-1977 and 2013-2014. In the spring and summer, the drying spread to the Midwest and Central Plains, driven by severe precipitation deficits downwind from regions of major dust storm activity, consistent with previous work linking drying during the Dust Bowl to anthropogenic dust aerosol forcing. Despite a moderate La Nina, contributions from sea surface temperature forcing were small, suggesting that the anomalous 1934 drought was primarily a consequence of atmospheric variability, possibly amplified by dust forcing that intensified and spread the drought across nearly all of western North America.
C1 [Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
   [Cook, Benjamin I.; Seager, Richard; Smerdon, Jason E.] Lamont Doherty Earth Observ, Palisades, NY USA.
RP Cook, BI (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM benjamin.i.cook@nasa.gov
RI Cook, Benjamin/H-2265-2012; Smerdon, Jason/F-9952-2011
FU NSF [AGS-1243204, AGS-1401400]; National Aeronautics and Space
   Administration Modeling Analysis and Prediction Program [WBS
   281945.02.04.02.74]
FX This work was supported by NSF awards AGS-1243204 ("Linking Near-term
   Future Changes in Weather and Hydroclimate in Western North America to
   Adaptation for Ecosystem and Water Management") and AGS-1401400
   ("Pan-Continental Drought Dynamics in Western North America").
   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"). NCDC drought data were downloaded from
   http://www1.ncdc.noaa.gov/pub/data/cmb/sotc/drought/2012/13/uspctarea-we
   tdry-mod.txt. NCEP-NCAR and Twentieth Century Reanalyses were obtained
   from the NOAA Earth System Research Laboratory
   (http://www.esrl.noaa.gov/psd/data/gridded/). CRU climate grids were
   downloaded from the British Atmospheric Data Centre
   (http://badc.nerc.ac.uk/home/index.html). HadISST data were provided by
   the Hadley Centre (http://www.metoffice.gov.uk/hadobs/hadisst/). The
   authors thank NASA Goddard Space Flight Center for providing the GEOS-5
   model results used in the analysis, two anonymous reviewers who provided
   valuable comments, and Edward R Cook of the Lamont-Doherty Earth
   Observatory for providing the version of the NADA used in this analysis.
   Lamont contribution 7835.
NR 37
TC 19
Z9 20
U1 14
U2 50
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 OCT 28
PY 2014
VL 41
IS 20
BP 7298
EP 7305
DI 10.1002/2014GL061661
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AU0WO
UT WOS:000345343100040
ER

PT J
AU Guan, B
   Waliser, DE
   Lee, T
   Halkides, DJ
AF Guan, Bin
   Waliser, Duane E.
   Lee, Tong
   Halkides, Daria J.
TI Influence of the Madden-Julian oscillation on the Indian Ocean
   cross-equatorial heat transport
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Madden-Julian oscillation; Indian Ocean; cross-equatorial heat transport
ID ATMOSPHERIC INTRASEASONAL VARIABILITY; GENERAL-CIRCULATION MODEL;
   TROPICAL CYCLONES; PACIFIC-OCEAN; KELVIN WAVES; MODULATION; SURFACE;
   MJO; SCALE; RECTIFICATION
AB The Indian Ocean cross-equatorial heat transport (CEHT) anomalies associated with the Madden-Julian oscillation (MJO) are analyzed using the National Centers for Environmental Prediction Climate Forecast System Reanalysis for the period 1979-2010. The magnitude of MJO-related CEHT anomalies, seasonal dependence, and interannual modulations are examined. The magnitude of composite MJO CEHT anomalies is similar to 30% (similar to 15%) of the amplitude of the seasonal climatology in winter (summer). Interannual modulation on average accounts for only similar to 10% of the total magnitude of intraseasonal variability of a given year. MJO CEHT is largely contributed by temperature flux anomalies in the upper similar to 140m, with notable compensation between two characteristic layers. The significance of MJO CEHT anomalies, the nonnegligible magnitude of residual CEHT accumulated from intraseasonal anomalies during specific years, and the vertical compensation of temperature flux anomalies that give rise to the CEHT, have implications to the potential importance of upper ocean thermodynamics in MJO evolution and regional climate.
C1 [Guan, Bin; Halkides, Daria J.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90045 USA.
   [Guan, Bin; Waliser, Duane E.; Lee, Tong; Halkides, Daria J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Guan, B (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90045 USA.
EM bin.guan@jpl.nasa.gov
RI Guan, Bin/F-6735-2010
NR 52
TC 0
Z9 0
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 28
PY 2014
VL 41
IS 20
BP 7314
EP 7322
DI 10.1002/2014GL061789
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA AU0WO
UT WOS:000345343100042
ER

PT J
AU van Diedenhoven, B
   Fridlind, AM
   Cairns, B
   Ackerman, AS
AF van Diedenhoven, Bastiaan
   Fridlind, Ann M.
   Cairns, Brian
   Ackerman, Andrew S.
TI Variation of ice crystal size, shape, and asymmetry parameter in tops of
   tropical deep convective clouds
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE ice clouds; ice crystals; deep convection; asymmetry parameter
ID SINGLE-SCATTERING PROPERTIES; MULTIDIRECTIONAL POLARIZATION
   MEASUREMENTS; SOLAR-RADIATION MEASUREMENTS; CIRRUS CLOUDS;
   OPTICAL-THICKNESS; MICROPHYSICAL PROPERTIES; SURFACE-ROUGHNESS;
   EFFECTIVE RADIUS; WESTERN PACIFIC; PARTICLE-SIZE
AB The variation of ice crystal properties in the tops of deep convective clouds off the north coast of Australia is analyzed. Cloud optical thickness, ice effective radius, aspect ratio of ice crystal components, crystal distortion parameter and asymmetry parameter are simultaneously retrieved from combined measurements of the Moderate Resolution Imaging Spectroradiometer (MODIS) and Polarization and Directionality of the Earth's Reflectances (POLDER) satellite instruments. The data are divided into periods with alternating weak and strong convection. Mostly plate-like particle components with aspect ratios closer to unity and lower asymmetry parameters characterize strongly convective periods, while weakly convective periods generally show lower aspect ratios, relatively more column-like shapes and somewhat greater asymmetry parameters. Results for strongly convective periods show that, with increasing cloud top temperature, the distortion parameter generally decreases, while the asymmetry parameter and effective radius increase. For one of the strongly convective periods, the rate at which effective radii increase with cloud top temperature is more than double that of the other periods, while the temperature dependence of the other microphysical quantities for this period is substantially weaker. Atmospheric state analysis indicates that these differences are concurrent with differences in middle-to-upper tropospheric zonal wind shear. The observed variation of microphysical properties may have significant effects on the shortwave radiative fluxes and cloud absorption associated with deep convection. Additionally, MODIS collection 5 effective radii are estimated to be biased small with an artificially narrow range. Collection 6 products are expected to have less severe biases that depend on cloud top temperature and atmospheric conditions.
C1 [van Diedenhoven, Bastiaan] Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA.
   [van Diedenhoven, Bastiaan; Fridlind, Ann M.; Cairns, Brian; Ackerman, Andrew S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP van Diedenhoven, B (reprint author), Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA.
EM bastiaan.vandiedenhoven@nasa.gov
RI Ackerman, Andrew/D-4433-2012; 
OI Ackerman, Andrew/0000-0003-0254-6253; van Diedenhoven,
   Bastiaan/0000-0001-5622-8619
FU NASA ROSES program [NNX11AG81G, NNX14AJ28G]
FX We would like to thank Christian Jacob of Monash University in
   Melbourne, Australia, for his comments on the work presented in this
   paper. We thank three anonymous reviewers for their contributions. The
   authors are grateful to Centre National d'Etudes Spatiales (CNES) and
   NASA for providing the POLDER and MODIS data. POLDER data were obtained
   through the ICARE Data and Services Center (www.icare.univ-lille1.fr).
   MODIS data are available at http://ladsweb.nascom.nasa.gov. NCEP data
   were provided by the NOAA-ESRL Physical Sciences Division, Boulder
   Colorado (www.esrl.noaa.gov/psd). TRMM data were obtained from the
   Giovanni online data system, developed, and maintained by the NASA GES
   DISC (http://disc.sci.gsfc.nasa.gov/giovanni). We are grateful to Bryan
   Baum at the University of Wisconsin-Madison for providing the ice
   particle size distributions
   (www.ssec.wisc.edu/ice_models/microphysical_data.html). This work is
   supported by the NASA ROSES program under grants NNX11AG81G and
   NNX14AJ28G.
NR 78
TC 9
Z9 9
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 OCT 27
PY 2014
VL 119
IS 20
BP 11809
EP 11825
DI 10.1002/2014JD022385
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AU0FE
UT WOS:000345298100020
ER

PT J
AU Roberge, A
AF Roberge, Aki
TI ASTRONOMY Hurling comets around a planetary nursery
SO NATURE
LA English
DT Editorial Material
ID BETA-PICTORIS; CIRCUMSTELLAR DISK; BODIES
C1 NASA, Goddard Space Flight Ctr, Exoplunets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
RP Roberge, A (reprint author), NASA, Goddard Space Flight Ctr, Exoplunets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
EM aki.roberge@nasa.gov
RI Roberge, Aki/D-2782-2012
OI Roberge, Aki/0000-0002-2989-3725
NR 8
TC 1
Z9 1
U1 0
U2 1
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 OCT 23
PY 2014
VL 514
IS 7523
BP 440
EP 441
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AR7RC
UT WOS:000343775900027
PM 25341780
ER

PT J
AU Peretyazhko, TS
   Zhang, QB
   Colvin, VL
AF Peretyazhko, Tanya S.
   Zhang, Qingbo
   Colvin, Vicki L.
TI Size-Controlled Dissolution of Silver Nanoparticles at Neutral and
   Acidic pH Conditions: Kinetics and Size Changes
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID ION RELEASE KINETICS; METAL-IONS; TOXICITY; OXYGEN; GENERATION;
   NANOSILVER; PARTICLES; AG
AB Silver nanoparticles (AgNP) are widely utilized in increasing number of medical and consumer products due to their antibacterial properties. Once released to aquatic system, AgNP undergoes oxidative dissolution leading to production of toxic Ag+. Dissolved Ag+ can have a severe impact on various organisms, including indigenous microbial communities, fungi, alga, plants, vertebrates, invertebrates, and human cells. Therefore, it is important to investigate fate of AgNP and determine physico-chemicals parameters that control AgNP behavior in the natural environment. Nanoparticle size might have a dominant effect on AgNP dissolution in natural waters. In this work, we investigated size-dependent dissolution of AgNP exposed to ultrapure deionized water (pH approximate to 7) and acetic acid (pH 3) and determined changes in nanoparticle size after dissolution. Silver nanoparticles stabilized by thiol functionalized methoxyl polyethylene glycol (PEGSH) of 6 nm (AgNP-6), 9 nm (AgNP-6), 13 nm (AgNP-13), and 70 nm (AgNP-70) were prepared. The results of dissolution experiments showed that the extent of AgNP dissolution in acetic acid was larger than in water. Solubility of AgNP increased with the size decrease and followed the order AgNP-6> AgNP-9 > AgNP-13 > AgNP-70 in both water and acetic acid. Transmission electron microscopy (TEM) was applied to characterize changes in size and morphology of the AgNP after dissolution in water. Analysis of AgNP by TEM revealed that the particle morphology did not change during dissolution. The particles remained approximately spherical in shape, and no visible aggregation was observed in the samples. TEM analysis also demonstrated that AgNP-6, AgNP-9, and AgNP-13 increased in size after dissolution likely due to Ostwald ripening.
C1 [Peretyazhko, Tanya S.; Zhang, Qingbo; Colvin, Vicki L.] Rice Univ, Dept Chem, Houston, TX 77005 USA.
RP Peretyazhko, TS (reprint author), NASA JSC, Jacobs, Houston, TX 77058 USA.
EM tanya.peretyazhko@nasa.gov
RI Zhang, Qingbo/B-7070-2015
OI Zhang, Qingbo/0000-0001-8289-0227
FU National Science Foundation [CMMI-1057906]
FX This research was supported by the National Science Foundation
   (CMMI-1057906).
NR 28
TC 52
Z9 52
U1 13
U2 144
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
EI 1520-5851
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD OCT 21
PY 2014
VL 48
IS 20
BP 11954
EP 11961
DI 10.1021/es50232021
PG 8
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA AR5RJ
UT WOS:000343640900026
PM 25265014
ER

PT J
AU Evans, A
   Gehrz, RD
   Woodward, CE
   Helton, LA
AF Evans, A.
   Gehrz, R. D.
   Woodward, C. E.
   Helton, L. A.
TI A WISE view of novae - I. The data
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; binaries: symbiotic; circumstellar matter; novae, cataclysmic
   variables; infrared: stars
ID SPITZER-SPACE-TELESCOPE; CLASSICAL NOVAE; CATACLYSMIC VARIABLES;
   INFRARED-SPECTROSCOPY; CASSIOPEIAE 1993; RS OPHIUCHI; ISO OBSERVATIONS;
   IRAS OBSERVATIONS; RECURRENT NOVAE; SILICATE DUST
AB We present the results of data-mining the Wide-field Infrared Survey Explorer (WISE) archive for data on classical and recurrent novae. We find that the detections are consistent with dust emission, line emission, emission by a stellar photosphere, or a combination of these. Of the 36 novae detected in one or more WISE bands, 16 are detected in all four; 31 known novae are not detected by WISE. We also searched for WISE data on post-WISE novae, to gain information about nova progenitors. In this first paper, we consider only the WISE data. In future papers, we will provide a more detailed modelling of the WISE data, and discuss WISE data on post-WISE novae
C1 [Evans, A.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
   [Gehrz, R. D.; Woodward, C. E.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
   [Helton, L. A.] USRA, SOFIA Sci Ctr, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Evans, A (reprint author), Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
EM a.evans@keele.ac.uk
FU NASA; United States Air Force; National Aeronautics and Space
   Administration
FX RDG was supported by NASA and the United States Air Force.; This
   publication makes use of data products from the WISE, which is a joint
   project of the University of California, Los Angeles, and the Jet
   Propulsion Laboratory/California Institute of Technology, funded by the
   National Aeronautics and Space Administration.
NR 89
TC 3
Z9 3
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 21
PY 2014
VL 444
IS 2
BP 1683
EP 1697
DI 10.1093/mnras/stu1467
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ6MF
UT WOS:000342926300050
ER

PT J
AU Pinfield, DJ
   Gromadzki, M
   Leggett, SK
   Gomes, J
   Lodieu, N
   Kurtev, R
   Day-Jones, AC
   Ruiz, MT
   Cook, NJ
   Morley, CV
   Marley, MS
   Marocco, F
   Smart, RL
   Jones, HRA
   Lucas, PW
   Beletsky, Y
   Ivanov, VD
   Burningham, B
   Jenkins, JS
   Cardoso, C
   Frith, J
   Clarke, JRA
   Galvez-Ortiz, MC
   Zhang, Z
AF Pinfield, D. J.
   Gromadzki, M.
   Leggett, S. K.
   Gomes, J.
   Lodieu, N.
   Kurtev, R.
   Day-Jones, A. C.
   Ruiz, M. T.
   Cook, N. J.
   Morley, C. V.
   Marley, M. S.
   Marocco, F.
   Smart, R. L.
   Jones, H. R. A.
   Lucas, P. W.
   Beletsky, Y.
   Ivanov, V. D.
   Burningham, B.
   Jenkins, J. S.
   Cardoso, C.
   Frith, J.
   Clarke, J. R. A.
   Galvez-Ortiz, M. C.
   Zhang, Z.
TI Discovery of a new Y dwarf: WISE J030449.03-270508.3
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; brown dwarfs; stars: low-mass
ID INFRARED-SURVEY-EXPLORER; THEORETICAL SPECTRAL MODELS; COOLEST BROWN
   DWARFS; DIGITAL SKY SURVEY; LARGE-AREA SURVEY; LOW-MASS STARS; T-DWARFS;
   SUBSTELLAR OBJECTS; GIANT PLANETS; BINARY-SYSTEM
AB We present a new Y dwarf, WISE J030449.03-270508.3, confirmed from a candidate sample designed to pick out low-temperature objects from the Wide-field Infrared Survey Explorer (WISE) data base. The new object is typed Y0pec following a visual comparison with spectral standards, and lies at a likely distance of 10-17 pc. Its tangential velocity suggests thin disc membership, but it shows some spectral characteristics that suggest that it may be metal poor and/or older than previously identified Y0 dwarfs. Based on trends seen for warmer late-type T dwarfs, the Y-band flux peak morphology is indicative of sub-solar metallicity, and the enhanced red wing of the J-band flux peak offers evidence for high gravity and/or low metallicity (with associated model trends suggesting an age closer to similar to 10 Gyr and mass in the range 0.02-0.03 M-circle dot). This object may thus be extending the population parameter space of the known Y0 dwarfs.
C1 [Pinfield, D. J.; Gomes, J.; Day-Jones, A. C.; Cook, N. J.; Marocco, F.; Jones, H. R. A.; Lucas, P. W.; Burningham, B.; Frith, J.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
   [Gromadzki, M.; Kurtev, R.; Clarke, J. R. A.] MAS, Santiago, Chile.
   [Gromadzki, M.; Kurtev, R.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso 2340000, Chile.
   [Leggett, S. K.] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA.
   [Lodieu, N.; Zhang, Z.] IAC, E-38200 Tenerife, Spain.
   [Lodieu, N.; Zhang, Z.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
   [Ruiz, M. T.; Jenkins, J. S.] Univ Chile, Dept Astron, Santiago, Chile.
   [Morley, C. V.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Marley, M. S.] NASA, Ames Res Ctr, Naval Air Stn, Mountain View, CA 94035 USA.
   [Smart, R. L.; Cardoso, C.] Osserv Astron Torino, Ist Nazl Astrofis, I-10025 Pino Torinese, Italy.
   [Beletsky, Y.] Carnegie Inst Sci, Las Campanas Observ, La Serena, Chile.
   [Ivanov, V. D.] ESO, Santiago 19, Chile.
   [Galvez-Ortiz, M. C.] Ctr Astrobiol CSIC INTA, E-28850 Madrid, Spain.
RP Pinfield, DJ (reprint author), Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
EM d.j.pinfield@herts.ac.uk
RI Jenkins, James/I-5284-2016; Ruiz, Maria Teresa/I-5770-2016; 
OI Burningham, Ben/0000-0003-4600-5627; Smart, Richard/0000-0002-4424-4766;
   Marley, Mark/0000-0002-5251-2943; Ruiz, Maria
   Teresa/0000-0002-6799-1537; Leggett, Sandy/0000-0002-3681-2989; Jones,
   Hugh/0000-0003-0433-3665; Ivanov, Valentin/0000-0002-5963-1283
FU National Aeronautics and Space Administration; RoPACS; RoPACS, a Marie
   Curie Initial Training Network - European Commission's Seventh Framework
   Programme; GEMINI-CONICYT Fund [32110014]; Gemini Observatory; Ramon y
   Cajal at the IAC in Tenerife [08-303-01-02]; national programme of the
   Spanish Ministry of Economy and Competitiveness (MINECO)
   [AYA2010-19136]; FONDECYT [1130140]; Fondecyt Postdoctorado [3100098];
   CONICYT [PB06]
FX This publication makes use of data products from the WISE, which is a
   joint project of the University of California, Los Angeles, and the Jet
   Propulsion Laboratory/California Institute of Technology, funded by the
   National Aeronautics and Space Administration. This paper includes data
   gathered with the 6.5 m Magellan Telescopes located at Las Campanas
   Observatory, Chile. 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 ppp.c-nnnn. DP, NL, and ADJ have received support from
   RoPACS during this research and JG was supported by RoPACS, a Marie
   Curie Initial Training Network funded by the European Commission's
   Seventh Framework Programme. MG is financed by the GEMINI-CONICYT Fund,
   allocated to the project 32110014. SKL is supported by the Gemini
   Observatory, which is operated by AURA, on behalf of the international
   Gemini partnership of Argentina, Australia, Brazil, Canada, Chile, the
   United Kingdom, and the United States of America. NL is a Ramon y Cajal
   at the IAC in Tenerife (fellowship number 08-303-01-02) and is funded by
   the national programme AYA2010-19136 of the Spanish Ministry of Economy
   and Competitiveness (MINECO). RK acknowledges partial support from
   FONDECYT through grant 1130140. ADJ was supported by a Fondecyt
   Postdoctorado under project number 3100098. MTR received support from
   PB06 (CONICYT). This research has made use of the SIMBAD data base,
   operated at CDS, Strasbourg, France.
NR 75
TC 11
Z9 11
U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 21
PY 2014
VL 444
IS 2
BP 1931
EP 1939
DI 10.1093/mnras/stu1540
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ6MF
UT WOS:000342926300076
ER

PT J
AU Chen, JR
   Numata, K
   Wu, ST
AF Chen, Jeffrey R.
   Numata, Kenji
   Wu, Stewart T.
TI Error reduction in retrievals of atmospheric species from symmetrically
   measured lidar sounding absorption spectra
SO OPTICS EXPRESS
LA English
DT Article
ID CO2 COLUMN ABSORPTION; CARBON-DIOXIDE; AIRBORNE MEASUREMENTS; LASER;
   MISSION; SPECTROMETER; REFLECTANCE; SENSITIVITY; PRECISION; NM
AB We report new methods for retrieving atmospheric constituents from symmetrically-measured lidar-sounding absorption spectra. The forward model accounts for laser line-center frequency noise and broadened line-shape, and is essentially linearized by linking estimated optical-depths to the mixing ratios. Errors from the spectral distortion and laser frequency drift are substantially reduced by averaging optical-depths at each pair of symmetric wavelength channels. Retrieval errors from measurement noise and model bias are analyzed parametrically and numerically for multiple atmospheric layers, to provide deeper insight. Errors from surface height and reflectance variations are reduced to tolerable levels by "averaging before log" with pulse-by-pulse ranging knowledge incorporated. (C) 2014 Optical Society of America
C1 [Chen, Jeffrey R.; Numata, Kenji; Wu, Stewart T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Numata, Kenji] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Chen, JR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM jeffrey.r.chen@nasa.gov
FU NASA Goddard Internal Research and Development program; NASA Earth
   Science Technology Office Instrument Incubator Program
FX The authors gratefully acknowledge Dr. J. Mao and Dr. X. Sun of NASA
   Goddard for fruitful discussions. They are also indebted to Dr. A.
   Amediek of Deutsches Zentrum fur Luft- und Raumfahrt (DLR) for sharing
   surface reflectance measurement data, Dr. J. Abshire and other members
   of the Goddard CO<INF>2</INF> sounder team for their support. This work
   was supported by the NASA Goddard Internal Research and Development
   program and the NASA Earth Science Technology Office Instrument
   Incubator Program.
NR 27
TC 3
Z9 3
U1 0
U2 3
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 OCT 20
PY 2014
VL 22
IS 21
BP 26055
EP 26075
DI 10.1364/OE.22.026055
PG 21
WC Optics
SC Optics
GA AS0ZF
UT WOS:000344004600143
PM 25401639
ER

PT J
AU Campbell, JF
   Lin, B
   Nehrir, AR
   Harrison, FW
   Obland, MD
AF Campbell, Joel F.
   Lin, Bing
   Nehrir, Amin R.
   Harrison, F. Wallace
   Obland, Michael D.
TI Binary phase shift keying on orthogonal carriers for multi-channel CO2
   absorption measurements in the presence of thin clouds
SO OPTICS EXPRESS
LA English
DT Article
ID COLUMN MEASUREMENTS; LASER SYSTEM; LIDAR
AB A new modulation technique for Continuous Wave (CW) Lidar is presented based on Binary Phase Shift Keying (BPSK) using orthogonal carriers closely spaced in frequency, modulated by Maximum Length (ML) sequences, which have a theoretical autocorrelation function with no sidelobes. This makes it possible to conduct multi-channel atmospheric differential absorption measurements in the presence of thin clouds without the need for further processing to remove errors caused by sidelobe interference while sharing the same modulation bandwidth. Flight tests were performed and data were collected using both BPSK and linear swept frequency modulation. This research shows there is minimal or no sidelobe interference in the presence of thin clouds for BPSK compared to linear swept frequency with significant sidelobe levels. Comparisons between of CO2 optical depth Signal to Noise (SNR) between the BPSK and linear swept frequency cases indicate a 21% drop in SNR for BPSK experimentally using the instrument under consideration. (C) 2014 Optical Society of America
C1 [Campbell, Joel F.; Lin, Bing; Nehrir, Amin R.; Harrison, F. Wallace; Obland, Michael D.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Campbell, JF (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM joel.f.campbell@nasa.gov
NR 12
TC 5
Z9 5
U1 0
U2 6
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 OCT 20
PY 2014
VL 22
IS 21
BP A1634
EP A1640
DI 10.1364/OE.22.0A1634
PG 7
WC Optics
SC Optics
GA AS0ZF
UT WOS:000344004600026
PM 25607320
ER

PT J
AU Ade, PAR
   Akiba, Y
   Anthony, AE
   Arnold, K
   Atlas, M
   Barron, D
   Boettger, D
   Borrill, J
   Chapman, S
   Chinone, Y
   Dobbs, M
   Elleflot, T
   Errard, J
   Fabbian, G
   Feng, C
   Flanigan, D
   Gilbert, A
   Grainger, W
   Halverson, NW
   Hasegawa, M
   Hattori, K
   Hazumi, M
   Holzapfel, WL
   Hori, Y
   Howard, J
   Hyland, P
   Inoue, Y
   Jaehnig, GC
   Jaffe, AH
   Keating, B
   Kermish, Z
   Keskitalo, R
   Kisner, T
   Le Jeune, M
   Lee, AT
   Leitch, EM
   Linder, E
   Lungu, M
   Matsuda, F
   Matsumura, T
   Meng, X
   Miller, NJ
   Morii, H
   Moyerman, S
   Myers, MJ
   Navaroli, M
   Nishino, H
   Orlando, A
   Paar, H
   Peloton, J
   Poletti, D
   Quealy, E
   Rebeiz, G
   Reichardt, CL
   Richards, PL
   Ross, C
   Schanning, I
   Schenck, DE
   Sherwin, BD
   Shimizu, A
   Shimmin, C
   Shimon, M
   Siritanasak, P
   Smecher, G
   Spieler, H
   Stebor, N
   Steinbach, B
   Stompor, R
   Suzuki, A
   Takakura, S
   Tomaru, T
   Wilson, B
   Yadav, A
   Zahn, O
AF Ade, P. A. R.
   Akiba, Y.
   Anthony, A. E.
   Arnold, K.
   Atlas, M.
   Barron, D.
   Boettger, D.
   Borrill, J.
   Chapman, S.
   Chinone, Y.
   Dobbs, M.
   Elleflot, T.
   Errard, J.
   Fabbian, G.
   Feng, C.
   Flanigan, D.
   Gilbert, A.
   Grainger, W.
   Halverson, N. W.
   Hasegawa, M.
   Hattori, K.
   Hazumi, M.
   Holzapfel, W. L.
   Hori, Y.
   Howard, J.
   Hyland, P.
   Inoue, Y.
   Jaehnig, G. C.
   Jaffe, A. H.
   Keating, B.
   Kermish, Z.
   Keskitalo, R.
   Kisner, T.
   Le Jeune, M.
   Lee, A. T.
   Leitch, E. M.
   Linder, E.
   Lungu, M.
   Matsuda, F.
   Matsumura, T.
   Meng, X.
   Miller, N. J.
   Morii, H.
   Moyerman, S.
   Myers, M. J.
   Navaroli, M.
   Nishino, H.
   Orlando, A.
   Paar, H.
   Peloton, J.
   Poletti, D.
   Quealy, E.
   Rebeiz, G.
   Reichardt, C. L.
   Richards, P. L.
   Ross, C.
   Schanning, I.
   Schenck, D. E.
   Sherwin, B. D.
   Shimizu, A.
   Shimmin, C.
   Shimon, M.
   Siritanasak, P.
   Smecher, G.
   Spieler, H.
   Stebor, N.
   Steinbach, B.
   Stompor, R.
   Suzuki, A.
   Takakura, S.
   Tomaru, T.
   Wilson, B.
   Yadav, A.
   Zahn, O.
CA Polarbear Collaboration
TI A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND B-MODE POLARIZATION
   POWER SPECTRUM AT SUB-DEGREE SCALES WITH POLARBEAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; large-scale
   structure of universe
ID PROBE WMAP OBSERVATIONS; ANGULAR SCALE; GRAVITY-WAVES; UPPER LIMIT; 20
   GHZ; CMB; EMISSION; MAPS; SUBMILLIMETER; CALIBRATION
AB We report a measurement of the B-mode polarization power spectrum in the cosmic microwave background (CMB) using the Polarbear experiment in Chile. The faint B-mode polarization signature carries information about the universe's entire history of gravitational structure formation, and the cosmic inflation that may have occurred in the very early universe. Our measurement covers the angular multipole range 500 < l < 2100 and is based on observations of an effective sky area of 25 deg(2) with 3 '.5 resolution at 150 GHz. On these angular scales, gravitational lensing of the CMB by intervening structure in the universe is expected to be the dominant source of B-mode polarization. Including both systematic and statistical uncertainties, the hypothesis of no B-mode polarization power from gravitational lensing is rejected at 97.2% confidence. The band powers are consistent with the standard cosmological model. Fitting a single lensing amplitude parameter A(BB) to the measured band powers, A(BB) = 1.12 +/- 0.61(stat)(-0.12)(+0.04)(sys) +/- 0.07(multi), where A(BB) = 1 is the fiducial wmap-9 Lambda CDM value. In this expression, "stat" refers to the statistical uncertainty, "sys" to the systematic uncertainty associated with possible biases from the instrument and astrophysical foregrounds, and "multi" to the calibration uncertainties that have a multiplicative effect on the measured amplitude A(BB).
C1 [Ade, P. A. R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3XQ, S Glam, Wales.
   [Akiba, Y.; Hasegawa, M.; Hazumi, M.; Inoue, Y.; Shimizu, A.] Grad Univ Adv Studies, Miura, Kanagawa 2400115, Japan.
   [Anthony, A. E.; Halverson, N. W.; Jaehnig, G. C.; Schenck, D. E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
   [Anthony, A. E.; Halverson, N. W.; Schenck, D. E.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
   [Arnold, K.; Atlas, M.; Barron, D.; Boettger, D.; Elleflot, T.; Feng, C.; Keating, B.; Matsuda, F.; Moyerman, S.; Orlando, A.; Paar, H.; Schanning, I.; Shimon, M.; Siritanasak, P.; Stebor, N.; Wilson, B.; Yadav, A.] Univ Calif San Diego, Dept Phys, San Diego, CA 92093 USA.
   [Borrill, J.; Errard, J.; Keskitalo, R.; Kisner, T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
   [Borrill, J.; Errard, J.; Kisner, T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Chapman, S.; Ross, C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada.
   [Chinone, Y.; Flanigan, D.; Holzapfel, W. L.; Howard, J.; Lee, A. T.; Lungu, M.; Meng, X.; Myers, M. J.; Quealy, E.; Reichardt, C. L.; Richards, P. L.; Sherwin, B. D.; Steinbach, B.; Suzuki, A.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
   [Chinone, Y.; Hasegawa, M.; Hattori, K.; Hazumi, M.; Hori, Y.; Matsumura, T.; Morii, H.; Takakura, S.; Tomaru, T.] KEK, High Energy Accelerator Res Org, Tsukuba, Ibaraki 3050801, Japan.
   [Dobbs, M.; Gilbert, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 0G4, Canada.
   [Fabbian, G.; Peloton, J.; Poletti, D.; Stompor, R.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, Obs Paris,Sorbonne Paris Cite, Paris, France.
   [Fabbian, G.] SISSA, Int Sch Adv Studies, I-34014 Trieste, Italy.
   [Flanigan, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
   [Grainger, W.] STFC, Rutherford Appleton Lab, Swindon SN2 1SZ, Wilts, England.
   [Halverson, N. W.; Jaehnig, G. C.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
   [Hazumi, M.; Nishino, H.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan.
   [Howard, J.] Univ Oxford, Dept Phys, Oxford OX1 2JD, England.
   [Hyland, P.] Dept Phys, Austin Coll, Sherman, TX 75090 USA.
   [Jaffe, A. H.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England.
   [Kermish, Z.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
   [Lee, A. T.; Linder, E.; Spieler, H.; Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
   [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.
   [Lungu, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
   [Miller, N. J.] NASA, Observ Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Quealy, E.] Napa Valley Coll, Dept Phys, Napa, CA 94558 USA.
   [Rebeiz, G.] Univ Calif San Diego, Dept Elect & Comp Engn, San Diego, CA 92093 USA.
   [Sherwin, B. D.] Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA.
   [Shimmin, C.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
   [Shimon, M.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
   [Smecher, G.] Three Speed Logic Inc, Vancouver, BC V6A 2J8, Canada.
   [Takakura, S.] Osaka Univ, Toyonaka, Osaka 5600043, Japan.
RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3XQ, S Glam, Wales.
RI Holzapfel, William/I-4836-2015; 
OI Orlando, Angiola/0000-0001-8004-5054
FU Department of Energy [DE-AC02-05CH11231]; National Science Foundation
   [AST-0618398, AST-1212230]; MEXT KAKENHI [21111002]; KEK Cryogenics
   Science Center; Natural Sciences and Engineering Research Council of
   Canada; Canada Research Chairs Program; Canadian Institute for Advanced
   Research; Miller Institute for Basic Research in Science; NASA; Simons
   Foundation; Joan and Irwin Jacobs; Comision Nacional de Investigacion
   Cientifica y Tecnologica de Chile (CONICYT)
FX Calculations were performed on the Central Computing System, owned and
   operated by the Computing Research Center at KEK, and the National
   Energy Research Scientific Computing Center, which is 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 KEK authors were supported by MEXT
   KAKENHI grant Number 21111002, and acknowledge support from KEK
   Cryogenics Science Center. The McGill authors acknowledge funding from
   the Natural Sciences and Engineering Research Council of Canada, the
   Canada Research Chairs Program, and Canadian Institute for Advanced
   Research. B.D.S. acknowledges support from the Miller Institute for
   Basic Research in Science, N.M. acknowledges support from the NASA
   Postdoctoral Program, and K.A. acknowledges support from the Simons
   Foundation. M.S. gratefully acknowledges support from Joan and Irwin
   Jacobs. All silicon wafer-based technology for POLARBEAR was fabricated
   at the UC Berkeley Nanolab. We are indebted to our Chilean team members,
   Nolberto Oyarce and Jose Cortes. The James Ax Observatory operates in
   the Parque Astronomic Atacama in Northern Chile under the auspices of
   the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile
   (CONICYT). Finally, we acknowledge the tremendous contributions by Huan
   Tran to the POLARBEAR project.
NR 78
TC 62
Z9 62
U1 2
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2014
VL 794
IS 2
AR 171
DI 10.1088/0004-637X/794/2/171
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8OF
UT WOS:000343085800075
ER

PT J
AU Arzoumanian, Z
   Brazier, A
   Burke-Spolaor, S
   Chamberlin, SJ
   Chatterjee, S
   Cordes, JM
   Demorest, PB
   Deng, X
   Dolch, T
   Ellis, JA
   Ferdman, RD
   Garver-Daniels, N
   Jenet, F
   Jones, G
   Kaspi, VM
   Koop, M
   Lam, MT
   Lazio, TJW
   Lommen, AN
   Lorimer, DR
   Luo, J
   Lynch, RS
   Madison, DR
   McLaughlin, MA
   McWilliams, ST
   Nice, DJ
   Palliyaguru, N
   Pennucci, TT
   Ransom, SM
   Sesana, A
   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.
   Cordes, J. M.
   Demorest, P. B.
   Deng, X.
   Dolch, T.
   Ellis, J. A.
   Ferdman, R. D.
   Garver-Daniels, N.
   Jenet, F.
   Jones, G.
   Kaspi, V. M.
   Koop, M.
   Lam, M. T.
   Lazio, T. J. W.
   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.
   Sesana, A.
   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 GRAVITATIONAL WAVES FROM INDIVIDUAL SUPERMASSIVE BLACK HOLE BINARIES IN
   CIRCULAR ORBITS: LIMITS FROM THE NORTH AMERICAN NANOHERTZ OBSERVATORY
   FOR GRAVITATIONAL WAVES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitation; pulsars: general
ID PULSAR TIMING ARRAYS; MILLISECOND PULSARS; COALESCENCE RATE; 3C 66B;
   RADIATION; GALAXIES; SYSTEMS; EVOLUTION; UNIVERSE; SEARCH
AB We perform a search for continuous gravitational waves from individual supermassive black hole binaries using robust frequentist and Bayesian techniques. We augment standard pulsar timing models with the addition of time-variable dispersion measure and frequency variable pulse shape terms. We apply our techniques to the Five Year Data Release from the North American Nanohertz Observatory for Gravitational Waves. We find that there is no evidence for the presence of a detectable continuous gravitational wave; however, we can use these data to place the most constraining upper limits to date on the strength of such gravitational waves. Using the full 17 pulsar data set we place a 95% upper limit on the strain amplitude of h(0) less than or similar to 3.0 x 10(-14) at a frequency of 10 nHz. Furthermore, we place 95% sky-averaged lower limits on the luminosity distance to such gravitational wave sources, finding that dL greater than or similar to 425 Mpc for sources at a frequency of 10 nHz and chirp mass 10(10) M-circle dot. We find that for gravitational wave sources near our best timed pulsars in the sky, the sensitivity of the pulsar timing array is increased by a factor of similar to four over the sky-averaged sensitivity. Finally we place limits on the coalescence rate of the most massive supermassive black hole binaries.
C1 [Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
   [Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
   [Brazier, A.; Chatterjee, S.; Cordes, J. M.; Dolch, T.; Lam, M. T.; Madison, D. R.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
   [Burke-Spolaor, S.] CALTECH, Pasadena, CA 91125 USA.
   [Chamberlin, S. J.; Ellis, J. A.; Siemens, X.] Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA.
   [Demorest, P. B.; Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
   [Deng, X.; Koop, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
   [Ferdman, R. D.; Kaspi, V. M.; Lynch, R. S.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
   [Garver-Daniels, N.; Lorimer, D. R.; McLaughlin, M. A.; McWilliams, S. T.; Palliyaguru, N.; Swiggum, J.] W Virginia Univ, Dept Phys, Morgantown, WV 26505 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.
   [Lazio, T. J. W.; Vallisneri, M.; van Haasteren, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
   [Lommen, A. N.] Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA.
   [Nice, D. J.] Lafayette Coll, Dept Phys, Easton, PA 18042 USA.
   [Pennucci, T. T.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
   [Sesana, A.; Zhu, W. W.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
   [Stairs, I. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
   [Stinebring, D. R.] Oberlin Coll, Dept Phys & Astron, Oberlin, OH 44074 USA.
   [Stovall, K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
RP Arzoumanian, Z (reprint author), NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Code 662, Greenbelt, MD 20771 USA.
RI Sesana, Alberto/Q-9826-2016; 
OI Sesana, Alberto/0000-0003-4961-1606; Nice, David/0000-0002-6709-2566;
   Ransom, Scott/0000-0001-5799-9714
FU National Science Foundation (NSF) PIRE program [0968296]; NSF [0923409,
   PHY-1307429, AST-1100968]; NSERC; NSF CAREER award [0955929]; Wisconsin
   Space Grant Consortium; NASA Einstein Fellowship [PF3-140116]
FX The authors thank Neil Cornish, Jolien Creighton, and Stephen Taylor for
   many useful discussions regarding the data analysis methods presented in
   this work. The work of Z.A., A.B., S.B.-S., S.J.C., S.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., A.N.L.,
   D.R.L., J.L., D.R.M., M.A.M., D.J.N., N.P., T.T.P., S.M.R., X.S.,
   D.R.S., K.S., J.S., and Y.W. was partially supported through the
   National Science Foundation (NSF) PIRE program award number 0968296. All
   computational work was performed on the Nemo cluster at UWM supported by
   NSF grant No. 0923409. NANOGrav research at UBC is supported by an NSERC
   Discovery Grant and Discovery Accelerator Supplement and by the Canadian
   Institute for Advanced Research. X.S. and J.E. were partially funded
   through an NSF CAREER award number 0955929 and through NSF grant No.
   PHY-1307429. J.E. was partially funded through the Wisconsin Space Grant
   Consortium. 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. 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. R.vH. is supported by NASA Einstein Fellowship grant
   PF3-140116.
NR 74
TC 36
Z9 36
U1 2
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2014
VL 794
IS 2
AR 141
DI 10.1088/0004-637X/794/2/141
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8OF
UT WOS:000343085800045
ER

PT J
AU Balokovic, M
   Comastri, A
   Harrison, FA
   Alexander, DM
   Ballantyne, DR
   Bauer, FE
   Boggs, SE
   Brandt, WN
   Brightman, M
   Christensen, FE
   Craig, WW
   Del Moro, A
   Gandhi, P
   Hailey, CJ
   Koss, M
   Lansbury, GB
   Luo, B
   Madejski, GM
   Marinucci, A
   Matt, G
   Markwardt, CB
   Puccetti, S
   Reynolds, CS
   Risaliti, G
   Rivers, E
   Stern, D
   Walton, DJ
   Zhang, WW
AF Balokovic, M.
   Comastri, A.
   Harrison, F. A.
   Alexander, D. M.
   Ballantyne, D. R.
   Bauer, F. E.
   Boggs, S. E.
   Brandt, W. N.
   Brightman, M.
   Christensen, F. E.
   Craig, W. W.
   Del Moro, A.
   Gandhi, P.
   Hailey, C. J.
   Koss, M.
   Lansbury, G. B. .
   Luo, B.
   Madejski, G. M.
   Marinucci, A.
   Matt, G.
   Markwardt, C. B.
   Puccetti, S.
   Reynolds, C. S.
   Risaliti, G.
   Rivers, E.
   Stern, D.
   Walton, D. J.
   Zhang, W. W.
TI THE NuSTAR VIEW OF NEARBY COMPTON-THICK ACTIVE GALACTIC NUCLEI: THE
   CASES OF NGC 424, NGC 1320, AND IC 2560
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 424, NGC 1320, IC 2560); galaxies: nuclei;
   galaxies: Seyfert; techniques: spectroscopic; X-rays: galaxies
ID SEYFERT 2 GALAXIES; RAY LUMINOSITY FUNCTION; XMM-NEWTON OBSERVATIONS;
   APPROXIMATE-TO 2; STAR-FORMATION; LINE REGION; SWIFT-BAT; MIDINFRARED
   SPECTROSCOPY; EDDINGTON RATIOS; TOLOLO 0109-383
AB We present X-ray spectral analyses for three Seyfert 2 active galactic nuclei (AGNs), NGC 424, NGC 1320, and IC 2560, observed by NuSTAR in the 3-79 keV band. The high quality hard X-ray spectra allow detailed modeling of the Compton reflection component for the first time in these sources. Using quasi-simultaneous NuSTAR and Swift/XRT data, as well as archival XMM-Newton data, we find that all three nuclei are obscured by Compton-thick material with column densities in excess of similar to 5 x 10(24) cm(-2), and that their X-ray spectra above 3 keV are dominated by reflection of the intrinsic continuum on Compton-thick material. Due to the very high obscuration, absorbed intrinsic continuum components are not formally required by the data in any of the sources. We constrain the intrinsic photon indices and the column density of the reflecting medium through the shape of the reflection spectra. Using archival multi-wavelength data we recover the intrinsic X-ray luminosities consistent with the broadband spectral energy distributions. Our results are consistent with the reflecting medium being an edge-on clumpy torus with a relatively large global covering factor and overall reflection efficiency of the order of 1%. Given the unambiguous confirmation of the Compton-thick nature of the sources, we investigate whether similar sources are likely to be missed by commonly used selection criteria for Compton-thick AGNs, and explore the possibility of finding their high-redshift counterparts.
C1 [Balokovic, M.; Harrison, F. A.; Rivers, E.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
   [Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
   [Alexander, D. M.; Del Moro, A.; Gandhi, P.; Lansbury, G. B. .] Univ Durham, Dept Phys, Durham DH1 3LE, England.
   [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
   [Bauer, F. E.] Pontificia Univ Catolica Chile 306, Fac Fis, Inst Astrofis, Santiago 22, Chile.
   [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
   [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
   [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
   [Brightman, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
   [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
   [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
   [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Koss, M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
   [Koss, M.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland.
   [Madejski, G. M.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
   [Marinucci, A.; Matt, G.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
   [Markwardt, C. B.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
   [Puccetti, S.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
   [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Reynolds, C. S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
   [Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
   [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Balokovic, M (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt,
   William/N-2844-2015; Comastri, Andrea/O-9543-2015; 
OI Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581;
   Brandt, William/0000-0002-0167-2453; Comastri,
   Andrea/0000-0003-3451-9970; Risaliti, Guido/0000-0002-3556-977X;
   Puccetti, Simonetta/0000-0002-2734-7835
FU International Fulbright Science and Technology Award; ASI-INAF
   [I/037/012/0-011/13]; Swiss National Science Foundation
   [PP00P2_138979/1]; NASA [NNG08FD60C]; National Aeronautics and Space
   Administration
FX The authors thank the anonymous referee for useful comments which have
   improved the manuscript. M.B. acknowledges support from the
   International Fulbright Science and Technology Award. A.C. acknowledges
   support from ASI-INAF grant I/037/012/0-011/13. M.K. gratefully
   acknowledges support from Swiss National Science Foundation Grant
   PP00P2_138979/1. This work was supported under NASA contract No.
   NNG08FD60C, and made use of data from the NuSTAR mission, a project led
   by the California Institute of Technology, managed by the Jet Propulsion
   Laboratory, and funded by the National Aeronautics and Space
   Administration. We thank the NuSTAR Operations, Software and Calibration
   teams for support with the execution and analysis of these observations.
   This research has made use of the NuSTAR Data Analysis Software
   (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC,
   Italy) and the California Institute of Technology (USA). This research
   made use of the XRT Data Analysis Software (XRTDAS), archival data,
   software and on-line services provided by the ASDC. This research has
   made use of NASA's Astrophysics Data System.
NR 102
TC 34
Z9 34
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 OCT 20
PY 2014
VL 794
IS 2
AR 111
DI 10.1088/0004-637X/794/2/111
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8OF
UT WOS:000343085800015
ER

PT J
AU Brandt, TD
   McElwain, MW
   Turner, EL
   Mede, K
   Spiegel, DS
   Kuzuhara, M
   Schlieder, JE
   Wisniewski, JP
   Abe, L
   Biller, B
   Brandner, W
   Carson, J
   Currie, T
   Egner, S
   Feldt, M
   Golota, T
   Goto, M
   Grady, CA
   Guyon, O
   Hashimoto, J
   Hayano, Y
   Hayashi, M
   Hayashi, S
   Henning, T
   Hodapp, KW
   Inutsuka, S
   Ishii, M
   Iye, M
   Janson, M
   Kandori, R
   Knapp, GR
   Kudo, T
   Kusakabe, N
   Kwon, J
   Matsuo, T
   Miyama, S
   Morino, JI
   Moro-Martin, A
   Nishimura, T
   Pyo, TS
   Serabyn, E
   Suto, H
   Suzuki, R
   Takami, M
   Takato, N
   Terada, H
   Thalmann, C
   Tomono, D
   Watanabe, M
   Yamada, T
   Takami, H
   Usuda, T
   Tamura, M
AF Brandt, Timothy D.
   McElwain, Michael W.
   Turner, Edwin L.
   Mede, Kyle
   Spiegel, David S.
   Kuzuhara, Masayuki
   Schlieder, Joshua E.
   Wisniewski, John P.
   Abe, L.
   Biller, B.
   Brandner, W.
   Carson, J.
   Currie, T.
   Egner, S.
   Feldt, M.
   Golota, T.
   Goto, M.
   Grady, C. A.
   Guyon, O.
   Hashimoto, J.
   Hayano, Y.
   Hayashi, M.
   Hayashi, S.
   Henning, T.
   Hodapp, K. W.
   Inutsuka, S.
   Ishii, M.
   Iye, M.
   Janson, M.
   Kandori, R.
   Knapp, G. R.
   Kudo, T.
   Kusakabe, N.
   Kwon, J.
   Matsuo, T.
   Miyama, S.
   Morino, J. -I.
   Moro-Martin, A.
   Nishimura, T.
   Pyo, T. -S.
   Serabyn, E.
   Suto, H.
   Suzuki, R.
   Takami, M.
   Takato, N.
   Terada, H.
   Thalmann, C.
   Tomono, D.
   Watanabe, M.
   Yamada, T.
   Takami, H.
   Usuda, T.
   Tamura, M.
TI A STATISTICAL ANALYSIS OF SEEDS AND OTHER HIGH-CONTRAST EXOPLANET
   SURVEYS: MASSIVE PLANETS OR LOW-MASS BROWN DWARFS?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; methods: statistical; open clusters and associations:
   general; planetary systems; stars: activity; stars: imaging
ID SUN-LIKE STARS; MAIN-SEQUENCE STARS; FINDING CAMPAIGN DISCOVERY;
   SCORPIUS-CENTAURUS COMPLEX; EXTRASOLAR GIANT PLANETS; DIRECT-IMAGING
   DISCOVERY; DEUTERIUM-BURNING LIMIT; PICTORIS MOVING GROUP; OC PROJECT
   ROTATION; YOUNG SOLAR ANALOGS
AB We conduct a statistical analysis of a combined sample of direct imaging data, totalling nearly 250 stars. The stars cover a wide range of ages and spectral types, and include five detections (kappa And b, two similar to 60 M-J brown dwarf companions in the Pleiades, PZ Tel B, and CD-35 2722B). For some analyses we add a currently unpublished set of SEEDS observations, including the detections GJ 504b and GJ 758B. We conduct a uniform, Bayesian analysis of all stellar ages using both membership in a kinematic moving group and activity/rotation age indicators. We then present a new statistical method for computing the likelihood of a substellar distribution function. By performing most of the integrals analytically, we achieve an enormous speedup over brute-force Monte Carlo. We use this method to place upper limits on the maximum semimajor axis of the distribution function derived from radialvelocity planets, finding model-dependent values of similar to 30-100 AU. Finally, we model the entire substellar sample, from massive brown dwarfs to a theoretically motivated cutoff at similar to 5 M-J, with a single power-law distribution. We find that p(M, a) alpha M-0.65 +/- 0.60 alpha(-0.85 +/- 0.39) (1 sigma errors) provides an adequate fit to our data, with 1.0%-3.1% (68% confidence) of stars hosting 5-70 M-J companions between 10 and 100 AU. This suggests that many of the directly imaged exoplanets known, including most (if not all) of the low-mass companions in our sample, formed by fragmentation in a cloud or disk, and represent the low-mass tail of the brown dwarfs.
C1 [Brandt, Timothy D.; Spiegel, David S.] Inst Adv Study, Princeton, NJ 08540 USA.
   [McElwain, Michael W.; Grady, C. A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
   [Turner, Edwin L.; Knapp, G. R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
   [Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Todai Inst Adv Study, Tokyo, Japan.
   [Mede, Kyle; Kuzuhara, Masayuki; Tamura, M.] Univ Tokyo, Tokyo, Japan.
   [Kuzuhara, Masayuki; Hashimoto, J.; Hayashi, S.; Iye, M.; Kandori, R.; Kudo, T.; Kusakabe, N.; Kwon, J.; Matsuo, T.; Morino, J. -I.; Suto, H.; Suzuki, R.; Tamura, M.] Natl Astron Observ Japan, Tokyo, Japan.
   [Kuzuhara, Masayuki] Tokyo Inst Technol, Tokyo 152, Japan.
   [Schlieder, Joshua E.; Brandner, W.; Feldt, M.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
   [Abe, L.] Lab Hippolyte Fizeau, Nice, France.
   [Biller, B.] Univ Edinburgh, Edinburgh, Midlothian, Scotland.
   [Carson, J.] Coll Charleston, Charleston, SC 29401 USA.
   [Currie, T.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
   [Egner, S.; Golota, T.; Guyon, O.; Hayano, Y.; Hayashi, S.; Ishii, M.; Nishimura, T.; Pyo, T. -S.; Takato, N.; Terada, H.; Tomono, D.; Takami, H.; Usuda, T.] Subaru Telescope, Hilo, HI USA.
   [Goto, M.] Univ Sternwarte Munchen, Munich, Germany.
   [Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
   [Inutsuka, S.] Nagoya Univ, Dept Phys, Nagoya, Aichi 464, Japan.
   [Janson, M.] Queens Univ Belfast, Belfast, Antrim, North Ireland.
   [Kwon, J.] Grad Univ Adv Studies, Dept Astron Sci, Tokyo, Japan.
   [Miyama, S.] Hiroshima Univ, Higashihiroshima 724, Japan.
   [Moro-Martin, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Serabyn, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
   [Thalmann, C.] ETH, Inst Astron, CH-8092 Zurich, Switzerland.
   [Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido, Japan.
   [Yamada, T.] Tohoku Univ, Astron Inst, Sendai, Miyagi 980, Japan.
RP Brandt, TD (reprint author), Inst Adv Study, Olden Lane, Princeton, NJ 08540 USA.
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
FU Corning Glass Works Foundation through a fellowship at the Institute for
   Advanced Study; World Premier International Research Center Initiative;
   MEXT, Japan; JSPS Research Fellowship for Young Scientists [25-8826];
   U.S. National Science Foundation [1009203]
FX This research is based on data collected at the Subaru Telescope, which
   is operated by the National Astronomical Observatories of Japan. T.D.B.
   gratefully acknowledges support from the Corning Glass Works Foundation
   through a fellowship at the Institute for Advanced Study. This research
   has been supported in part by the World Premier International Research
   Center Initiative, MEXT, Japan. M.K. acknowledges support from a JSPS
   Research Fellowship for Young Scientists (grant no. 25-8826). J.C. was
   supported by the U.S. National Science Foundation under award no.
   1009203. This research has made use of the SIMBAD database and Vizier
   service, operated at CDS, Strasbourg, France. The authors wish to
   recognize and acknowledge the very significant cultural role and
   reverence that the summit of Mauna Kea has always had within the
   indigenous Hawaiian community. We are most fortunate to have the
   opportunity to conduct observations from this mountain.
NR 175
TC 37
Z9 37
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 OCT 20
PY 2014
VL 794
IS 2
AR 159
DI 10.1088/0004-637X/794/2/159
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8OF
UT WOS:000343085800063
ER

PT J
AU Donahue, M
   Voit, GM
   Mahdavi, A
   Umetsu, K
   Ettori, S
   Merten, J
   Postman, M
   Hoffer, A
   Baldi, A
   Coe, D
   Czakon, N
   Bartelmann, M
   Benitez, N
   Bouwens, R
   Bradley, L
   Broadhurst, T
   Ford, H
   Gastaldello, F
   Grillo, C
   Infante, L
   Jouvel, S
   Koekemoer, A
   Kelson, D
   Lahav, O
   Lemze, D
   Medezinski, E
   Melchior, P
   Meneghetti, M
   Molino, A
   Moustakas, J
   Moustakas, LA
   Nonino, M
   Rosati, P
   Sayers, J
   Seitz, S
   Van der Wel, A
   Zheng, W
   Zitrin, A
AF Donahue, Megan
   Voit, G. Mark
   Mahdavi, Andisheh
   Umetsu, Keiichi
   Ettori, Stefano
   Merten, Julian
   Postman, Marc
   Hoffer, Aaron
   Baldi, Alessandro
   Coe, Dan
   Czakon, Nicole
   Bartelmann, Mattias
   Benitez, Narciso
   Bouwens, Rychard
   Bradley, Larry
   Broadhurst, Tom
   Ford, Holland
   Gastaldello, Fabio
   Grillo, Claudio
   Infante, Leopoldo
   Jouvel, Stephanie
   Koekemoer, Anton
   Kelson, Daniel
   Lahav, Ofer
   Lemze, Doron
   Medezinski, Elinor
   Melchior, Peter
   Meneghetti, Massimo
   Molino, Alberto
   Moustakas, John
   Moustakas, Leonidas A.
   Nonino, Mario
   Rosati, Piero
   Sayers, Jack
   Seitz, Stella
   Van der Wel, Arjen
   Zheng, Wei
   Zitrin, Adi
TI CLASH-X: A COMPARISON OF LENSING AND X-RAY TECHNIQUES FOR MEASURING THE
   MASS PROFILES OF GALAXY CLUSTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmological parameters; dark matter; galaxies: clusters: intracluster
   medium; gravitational lensing: strong; gravitational lensing: weak;
   X-rays: galaxies: clusters
ID XMM-NEWTON; TEMPERATURE RELATION; SUNYAEV-ZELDOVICH; SCALING RELATIONS;
   DARK-MATTER; COSMOLOGICAL CONSTRAINTS; INTRACLUSTER MEDIUM; RXC
   J2248.7-4431; MACS J1206.2-0847; SUPERNOVA SURVEY
AB We present profiles of temperature, gas mass, and hydrostatic mass estimated from new and archival X-ray observations ofCLASHclusters. We comparemeasurements derived fromXMMand Chandra observations with one another and compare both to gravitational lensing mass profiles derived with CLASH Hubble Space Telescope and Subaru Telescope lensing data. Radial profiles of Chandra andXMMmeasurements of electron density and enclosed gasmass are nearly identical, indicating that differences in hydrostatic masses inferred fromX-ray observations arise from differences in gas-temperature measurements. Encouragingly, gas temperatures measured in clusters by XMM and Chandra are consistent with one another at similar to 100-200 kpc radii, but XMM temperatures systematically decline relative to Chandra temperatures at larger radii. The angular dependence of the discrepancy suggests that additional investigation on systematics such as the XMM point-spread function correction, vignetting, and off-axis responses is yet required. We present the CLASH-X mass-profile comparisons in the form of cosmology-independent and redshift-independent circular-velocity profiles. We argue that comparisons of circular-velocity profiles are the most robust way to assess mass bias. Ratios of Chandra hydrostatic equilibrium (HSE) mass profiles to CLASH lensing profiles show no obvious radial dependence in the 0.3-0.8 Mpc range. However, the mean mass biases inferred from the weak-lensing (WL) and SaWLens data are different. As an example, the weighted-mean value at 0.5 Mpc is < b > = 0.12 for the WL comparison and < b > = -0.11 for the SaWLens comparison. The ratios of XMM HSE mass profiles to CLASH lensing profiles show a pronounced radial dependence in the 0.3-1.0 Mpc range, with a weighted mean mass bias value rising to < b > greater than or similar to 0.3 at similar to 1 Mpc for the WL comparison and < b > approximate to 0.25 for the SaWLens comparison. The enclosed gas mass profiles from both Chandra and XMM rise to a value approximate to 1/8 times the total-mass profiles inferred from lensing at approximate to 0.5 Mpc and remain constant outside of that radius, suggesting that M-gas x 8 profiles may be an excellent proxy for total-mass profiles at greater than or similar to 0.5 Mpc in massive galaxy clusters.
C1 [Donahue, Megan; Voit, G. Mark; Hoffer, Aaron; Baldi, Alessandro] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
   [Mahdavi, Andisheh] San Francisco State Univ, San Francisco, CA 94132 USA.
   [Umetsu, Keiichi; Czakon, Nicole] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
   [Umetsu, Keiichi; Czakon, Nicole] Osservatorio Astron Bologna, I-40127 Bologna, Italy.
   [Ettori, Stefano; Meneghetti, Massimo] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy.
   [Merten, Julian; Meneghetti, Massimo; Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Postman, Marc; Coe, Dan; Bradley, Larry; Koekemoer, Anton; Lemze, Doron; Medezinski, Elinor] STScI, Baltimore, MD 21218 USA.
   [Bartelmann, Mattias] Heidelberg Univ, Zentrum Astron, D-69120 Heidelberg, Germany.
   [Benitez, Narciso] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
   [Broadhurst, Tom] Univ Basque Country, Dept Theoret Phys, E-48080 Bilbao, Spain.
   [Ford, Holland; Jouvel, Stephanie; Zheng, Wei] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
   [Lahav, Ofer] UCL, Dept Phys & Astron, London WC1E 6BT, England.
   [Molino, Alberto] Inst Astrofis Andalucia, E-18008 Granada, Spain.
   [Rosati, Piero] Univ Ferrara, Dept Phys & Astron, I-44122 Ferrara, Italy.
   [Sayers, Jack; Zitrin, Adi] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
   [Bouwens, Rychard] Leiden Observ, NL-2333 CA Leiden, Netherlands.
   [Infante, Leopoldo] Pontificia Univ Catolica Chile, Dept Astron Astrofis, Santiago 22, Chile.
   [Gastaldello, Fabio] INAF IASF, I-20133 Milan, Italy.
   [Kelson, Daniel] Carnegie Observ, Pasadena, CA 91101 USA.
   [Melchior, Peter] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
   [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA.
   [Nonino, Mario] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy.
   [Gastaldello, Fabio] Univ Calif Irvine, Irvine, CA 92697 USA.
   [Seitz, Stella] Univ Sternwarte Munchen, Dept Phys, D-81679 Munich, Germany.
   [Van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Grillo, Claudio] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
RP Donahue, M (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
EM donahue@pa.msu.edu
RI Grillo, Claudio/E-6223-2015; Gastaldello, Fabio/N-4226-2015; Ettori,
   Stefano/N-5004-2015; Meneghetti, Massimo/O-8139-2015; 
OI Grillo, Claudio/0000-0002-5926-7143; Umetsu,
   Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360;
   Koekemoer, Anton/0000-0002-6610-2048; Gastaldello,
   Fabio/0000-0002-9112-0184; Ettori, Stefano/0000-0003-4117-8617;
   Meneghetti, Massimo/0000-0003-1225-7084; Nonino,
   Mario/0000-0001-6342-9662; Benitez, Narciso/0000-0002-0403-7455;
   Donahue, Megan/0000-0002-2808-0853; Voit, Gerard/0000-0002-3514-0383
FU STScI/NASA award [HST-GO-12065.07-A]; NASA [NNX13AI41G]; DNRF; NASA ADAP
   award [NNX12AE45G]; ASI-INAF [I/023/05/0, I/088/06/0]; NASA; project
   INFN PD51 [ASI/INAF I/023/12/0]; NASA through a Hubble Fellowship grant
   [HST-HF-51334.01-A]; STScI
FX M.D. and A.H. acknowledge the partial support of STScI/NASA award
   HST-GO-12065.07-A and NASA award NNX13AI41G. M.D. and G.M.V. benefitted
   from discussions of this work with Jim Bartlett. The Dark Cosmology
   Centre is funded by the DNRF. A.M. was partially supported through NASA
   ADAP award NNX12AE45G. S.E. acknowledges the financial contribution from
   contracts ASI-INAF I/023/05/0 and I/088/06/0. The work of L.A.M. and
   J.M. was carried out at Jet Propulsion Laboratory, California Institute
   of Technology, under a contract with NASA. M.M. acknowledges financial
   contribution from the agreement ASI/INAF I/023/12/0 and from the project
   INFN PD51. Support for A.Z. is provided by NASA through a Hubble
   Fellowship grant HST-HF-51334.01-A awarded by STScI.
NR 86
TC 38
Z9 38
U1 1
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2014
VL 794
IS 2
AR 136
DI 10.1088/0004-637X/794/2/136
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8OF
UT WOS:000343085800040
ER

PT J
AU Freeman, M
   Montez, R
   Kastner, JH
   Balick, B
   Frew, DJ
   Jones, D
   Miszalski, B
   Sahai, R
   Blackman, E
   Chu, YH
   De Marco, O
   Frank, A
   Guerrero, MA
   Lopez, JA
   Zijlstra, A
   Bujarrabal, V
   Corradi, RLM
   Nordhaus, J
   Parker, QA
   Sandin, C
   Schonberner, D
   Soker, N
   Sokoloski, JL
   Steffen, M
   Toala, JA
   Ueta, T
   Villaver, E
AF Freeman, M.
   Montez, R., Jr.
   Kastner, J. H.
   Balick, B.
   Frew, D. J.
   Jones, D.
   Miszalski, B.
   Sahai, R.
   Blackman, E.
   Chu, Y. -H.
   De Marco, O.
   Frank, A.
   Guerrero, M. A.
   Lopez, J. A.
   Zijlstra, A.
   Bujarrabal, V.
   Corradi, R. L. M.
   Nordhaus, J.
   Parker, Q. A.
   Sandin, C.
   Schoenberner, D.
   Soker, N.
   Sokoloski, J. L.
   Steffen, M.
   Toala, J. A.
   Ueta, T.
   Villaver, E.
TI THE CHANDRA PLANETARY NEBULA SURVEY (CHANPLANS). II. X-RAY EMISSION FROM
   COMPACT PLANETARY NEBULAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; planetary nebulae: individual (NGC 1501, NGC 3918,
   NGC 6153, NGC 6369, HbDs 1, NGC 6337, Sp 1); stars: AGB and post-AGB
ID BINARY CENTRAL STAR; H-ALPHA SURVEY; TIME SEQUENCE O; MASSIVE STARS;
   COMMON-ENVELOPE; MAGNETIC-FIELDS; WOLF-RAYET; CIRCUMSTELLAR GAS; HOT
   BUBBLE; DYNAMICAL EVOLUTION
AB We present results from the most recent set of observations obtained as part of the Chandra X-ray observatory Planetary Nebula Survey (ChanPlaNS), the first comprehensive X-ray survey of planetary nebulae (PNe) in the solar neighborhood (i.e., within similar to 1.5 kpc of the Sun). The survey is designed to place constraints on the frequency of appearance and range of X-ray spectral characteristics of X-ray-emitting PN central stars and the evolutionary timescales of wind-shock-heated bubbles within PNe. ChanPlaNS began with a combined Cycle 12 and archive Chandra survey of 35 PNe. ChanPlaNS continued via a Chandra Cycle 14 Large Program which targeted all (24) remaining known compact (R-neb less than or similar to 0.4 pc), young PNe that lie within similar to 1.5 kpc. Results from these Cycle 14 observations include first-time X-ray detections of hot bubbles within NGC 1501, 3918, 6153, and 6369, and point sources in HbDs 1, NGC 6337, and Sp 1. The addition of the Cycle 14 results brings the overall ChanPlaNS diffuse X-ray detection rate to similar to 27% and the point source detection rate to similar to 36%. It has become clearer that diffuse X-ray emission is associated with young (less than or similar to 5 x 10(3) yr), and likewise compact (R-neb less than or similar to 0.15 pc), PNe with closed structures and high central electron densities (n(e) greater than or similar to 1000 cm(-3)), and is rarely associated with PNe that show H-2 emission and/or pronounced butterfly structures. Hb 5 is one such exception of a PN with a butterfly structure that hosts diffuse X-ray emission. Additionally, two of the five new diffuse X-ray detections (NGC 1501 and NGC 6369) host [WR]-type central stars, supporting the hypothesis that PNe with central stars of [WR]-type are likely to display diffuse X-ray emission.
C1 [Freeman, M.; Kastner, J. H.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
   [Freeman, M.; Kastner, J. H.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA.
   [Montez, R., Jr.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
   [Balick, B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
   [Frew, D. J.; De Marco, O.; Parker, Q. A.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia.
   [Frew, D. J.; De Marco, O.; Parker, Q. A.] Macquarie Univ, Macquarie Res Ctr Astron Astrophys & Astrophoton, Sydney, NSW 2109, Australia.
   [Jones, D.] Univ Atacama, Dept Fis, Copiapo, Chile.
   [Jones, D.] European So Observ, Santiago 19, Chile.
   [Miszalski, B.] S African Astron Observ, ZA-7935 Observatory, South Africa.
   [Miszalski, B.] Southern African Large Telescope Fdn, ZA-7935 Observatory, South Africa.
   [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Blackman, E.; Frank, A.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
   [Chu, Y. -H.] Univ Illinois, Dept Astron, Urbana, IL USA.
   [Guerrero, M. A.; Toala, J. A.] IAA CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
   [Lopez, J. A.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico.
   [Zijlstra, A.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
   [Bujarrabal, V.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
   [Corradi, R. L. M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
   [Corradi, R. L. M.; Nordhaus, J.] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 USA.
   [Parker, Q. A.] Australian Astron Observ, Epping, NSW 2121, Australia.
   [Sandin, C.; Schoenberner, D.; Steffen, M.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
   [Soker, N.] Observ Astron Nacl, E-28803 Alcala De Henares, Spain.
   [Sokoloski, J. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Ueta, T.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
   [Villaver, E.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
RP Freeman, M (reprint author), Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA.
RI Jones, David/G-8109-2014; 
OI Jones, David/0000-0003-3947-5946; Guerrero, Martin/0000-0002-7759-106X;
   Balick, Bruce/0000-0002-3139-3201; Frew, David/0000-0002-3108-5284
FU Chandra X-ray Observatory Center [GO3-14019A]; NASA [NAS8-03060];
   Spanish MICINN [AYA 2011-29754-C03-02]; FEDER; STScI under U.S.
   Government [NAG W-2166]
FX We thank the anonymous referee for helpful comments. This research was
   supported via award No. GO3-14019A to RIT issued by the Chandra X-ray
   Observatory Center, which is operated by the Smithsonian Astrophysical
   Observatory for and on behalf of NASA under contract NAS8-03060. Jesus
   A. Toala and Martin A. Guerrero are supported by the Spanish MICINN
   grant AYA 2011-29754-C03-02 co-funded with FEDER funds. The Digitized
   Sky Surveys were produced at STScI under U.S. Government Grant NAG
   W-2166. This research has also made use of the SIMBAD database, operated
   at CDS, Strasbourg, France.
NR 85
TC 11
Z9 11
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2014
VL 794
IS 2
AR 99
DI 10.1088/0004-637X/794/2/99
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8OF
UT WOS:000343085800003
ER

PT J
AU Gagliuffi, DCB
   Burgasser, AJ
   Gelino, CR
   Looper, DL
   Nicholls, CP
   Schmidt, SJ
   Cruz, K
   West, AA
   Gizis, JE
   Metchev, S
AF Gagliuffi, Daniella C. Bardalez
   Burgasser, Adam J.
   Gelino, Christopher R.
   Looper, Dagny L.
   Nicholls, Christine P.
   Schmidt, Sarah J.
   Cruz, Kelle
   West, Andrew A.
   Gizis, John E.
   Metchev, Stanimir
TI SpeX SPECTROSCOPY OF UNRESOLVED VERY LOW MASS BINARIES. II.
   IDENTIFICATION OF 14 CANDIDATE BINARIES WITH LATE-M/EARLY-L AND T DWARF
   COMPONENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; binaries: general; brown dwarfs; stars: low-mass
ID DIGITAL SKY SURVEY; HIGH PROPER-MOTION; NEAR-INFRARED SPECTRA; YOUNG
   BROWN DWARFS; ULTRA-COOL DWARFS; PECULIAR L DWARFS; FIELD L-DWARFS; BLUE
   L DWARF; L/T TRANSITION; OPTICAL SPECTROSCOPY
AB Multiplicity is a key statistic for understanding the formation of very low mass (VLM) stars and brown dwarfs. Currently, the separation distribution of VLM binaries remains poorly constrained at small separations (<= 1 AU), leading to uncertainty in the overall binary fraction. We approach this problem by searching for late-M/early-L plus T dwarf spectral binaries whose combined light spectra exhibit distinct peculiarities, allowing for separation-independent identification. We define a set of spectral indices designed to identify these systems, and we use a spectral template fitting method to confirm and characterize spectral binary candidates from a library of 815 spectra from the SpeX Prism Spectral Libraries. We present 11 new binary candidates, confirm 3 previously reported candidates, and rule out 2 previously identified candidates, all with primary and secondary spectral types in the range M7-L7 and T1-T8, respectively. We find that subdwarfs and blue L dwarfs are the primary contaminants in our sample and propose a method for segregating these sources. If confirmed by follow-up observations, these systems may add to the growing list of tight separation binaries, whose orbital properties may yield further insight into brown dwarf formation scenarios.
C1 [Gagliuffi, Daniella C. Bardalez; Burgasser, Adam J.; Nicholls, Christine P.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
   [Gelino, Christopher R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
   [Gelino, Christopher R.] NYU, Tisch Sch Arts, New York, NY 10003 USA.
   [Looper, Dagny L.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia.
   [Nicholls, Christine P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
   [Schmidt, Sarah J.] CUNY Hunter Coll, Dept Phys & Astron, New York, NY 10065 USA.
   [Cruz, Kelle] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
   [Cruz, Kelle] Boston Univ, Dept Astron, Boston, MA 02215 USA.
   [West, Andrew A.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
   [Gizis, John E.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
   [Metchev, Stanimir] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
RP Gagliuffi, DCB (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr,Mail Code 0424, La Jolla, CA 92093 USA.
EM daniella@physics.ucsd.edu
OI Schmidt, Sarah/0000-0002-7224-7702; Gizis, John/0000-0002-8916-1972
FU International Center at UCSD
FX The authors thank telescope operators for their assistance during the
   observations. D.B.G. would like to thank the Friends of the
   International Center at UCSD for their generous scholarship, as well as
   Davy Kirkpatrick and fellow graduate students Alex Mendez and David
   Vidmar for their helpful discussion and coding tips. This publication
   makes use of data from the SpeX Prism Spectral Libraries, maintained by
   Adam Burgasser at http://www.browndwarfs.org/spexprism, the Dwarf
   Archives Compendium, maintained by Chris Gelino at
   http://DwartArehives.org, and the VLM Binaries Archive, maintained by
   Nick Siegler at Mip://vlmbinaries.org. The authors wish to recognize and
   acknowledge the very significant cultural role and reverence that the
   summit of Mauna Kea has always had within the indigenous Hawaiian
   community. We are most fortunate to have the opportunity to conduct
   observations from this mountain.
NR 162
TC 22
Z9 22
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 OCT 20
PY 2014
VL 794
IS 2
AR 143
DI 10.1088/0004-637X/794/2/143
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8OF
UT WOS:000343085800047
ER

PT J
AU Gandhi, P
   Lansbury, GB
   Alexander, DM
   Stern, D
   Arevalo, P
   Ballantyne, DR
   Balokovic, M
   Bauer, FE
   Boggs, SE
   Brandt, WN
   Brightman, M
   Christensen, FE
   Comastri, A
   Craig, WW
   Del Moro, A
   Elvis, M
   Fabian, AC
   Hailey, CJ
   Harrison, FA
   Hickox, RC
   Koss, M
   LaMassa, SM
   Luo, B
   Madejski, GM
   Ptak, AF
   Puccetti, S
   Teng, SH
   Urry, CM
   Walton, DJ
   Zhang, WW
AF Gandhi, P.
   Lansbury, G. B.
   Alexander, D. M.
   Stern, D.
   Arevalo, P.
   Ballantyne, D. R.
   Balokovic, M.
   Bauer, F. E.
   Boggs, S. E.
   Brandt, W. N.
   Brightman, M.
   Christensen, F. E.
   Comastri, A.
   Craig, W. W.
   Del Moro, A.
   Elvis, M.
   Fabian, A. C.
   Hailey, C. J.
   Harrison, F. A.
   Hickox, R. C.
   Koss, M.
   LaMassa, S. M.
   Luo, B.
   Madejski, G. M.
   Ptak, A. F.
   Puccetti, S.
   Teng, S. H.
   Urry, C. M.
   Walton, D. J.
   Zhang, W. W.
TI NuSTAR UNVEILS A COMPTON-THICK TYPE 2 QUASAR IN MrK 34 (vol 792, pg 117,
   2014)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
ID GALAXY; SUZAKU
C1 [Gandhi, P.; Lansbury, G. B.; Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
   [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Arevalo, P.; Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
   [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile.
   [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
   [Balokovic, M.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
   [Bauer, F. E.] Millennium Inst Astrophys, Santiago, Chile.
   [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
   [Boggs, S. E.; Luo, B.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
   [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
   [Brightman, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
   [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
   [Comastri, A.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
   [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
   [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
   [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
   [Koss, M.] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
   [LaMassa, S. M.; Urry, C. M.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
   [Madejski, G. M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
   [Ptak, A. F.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
   [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy.
   [Puccetti, S.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy.
   [Teng, S. H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
RP Gandhi, P (reprint author), Univ Durham, Dept Phys, S Rd, Durham DH1 3LE, England.
EM poshak.gandhi@durham.ac.uk
RI Boggs, Steven/E-4170-2015; Brandt, William/N-2844-2015
OI Boggs, Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453
NR 12
TC 1
Z9 1
U1 1
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2014
VL 794
IS 2
AR 176
DI 10.1088/0004-637X/794/2/176
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8OF
UT WOS:000343085800080
ER

PT J
AU Lau, RM
   Herter, TL
   Morris, MR
   Adams, JD
AF Lau, R. M.
   Herter, T. L.
   Morris, M. R.
   Adams, J. D.
TI DUSTY CRADLES IN A TURBULENT NURSERY: THE SGR A EAST H II REGION COMPLEX
   AT THE GALACTIC CENTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: center; H II regions; infrared: ISM
ID PASCHEN-ALPHA SURVEY; EMISSION-LINE STARS; TEMPERATURE-FLUCTUATIONS;
   INTERSTELLAR GRAINS; MIDINFRARED CAMERA; DATA REDUCTION; EXTINCTION;
   SOFIA/FORCAST; CALIBRATION; FORCAST
AB We present imaging at 19, 25, 31, and 37 mu m of the compact H II region complex G-0.02-0.07 located 6 pc in projection from the center of the Galaxy obtained with SOFIA using FORCAST. G-0.02-0.07 contains three compact H II regions (A, B, and C) and one ultra-compact H II region (D). Our observations reveal the presence of two faint, infrared sources located 23 '' and 35 '' to the east of region C (FIRS 1 and 2) and detect dust emission in two of the three "ridges" of ionized gas west of region A. The 19/37 color temperature and 37 mu m optical depth maps of regions A-C are used to characterize the dust energetics and morphology. Regions A and B exhibit average 19/37 color temperatures of similar to 105 K, and regions C and D exhibit color temperatures of similar to 115K and similar to 130 K, respectively. Using the DustEM code, we model the SEDs of regions A-D and FIRS 1, all of which require populations of very small, transiently heated grains and large, equilibrium-heated grains. We also require the presence of polycyclic aromatic hydrocarbons in regions A-C in order to fit the 3.6, 4.5, 5.8, and 8.0 mu m fluxes observed by Spitzer/IRAC. The location of the heating source for region A is determined by triangulation from distances and temperatures derived from DustEM models fit to SEDs of three different points around the region, and it is found to be displaced to the northeast of the center of curvature near the color temperature peak. Based on total luminosity, expected 1.90 mu m fluxes, and proximity to the mid-IR color temperature peaks, we identify heating source candidates for regions A, B, and C. However, for region D, the observed fluxes at 1.87 and 1.90 mu m of the previously proposed ionizing star are a factor of similar to 40 times too bright to be the heating source and hence is likely just a star lying along the line of sight toward region D.
C1 [Lau, R. M.; Herter, T. L.; Adams, J. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
   [Morris, M. R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
   [Adams, J. D.] Univ Space Res Assoc, NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
RP Lau, RM (reprint author), Cornell Univ, Dept Astron, 202 Space Sci Bldg, Ithaca, NY 14853 USA.
FU Universities Space Research Association, Inc. (USRA), under NASA
   [NAS2-97001]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901];
   NASA through USRA [8500-98-014]
FX We thank the rest of the FORCAST team, George Gull, Justin Schoenwald,
   and Chuck Henderson, the USRA Science and Mission Ops teams, and the
   entire SOFIA staff. We would also like to thank Betsy Mills for her
   valuable comments. This work is based on observations made with the
   NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA
   science mission operations are conducted jointly by the Universities
   Space Research Association, Inc. (USRA), under NASA contract NAS2-97001,
   and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901.
   Financial support for FORCAST was provided by NASA through award
   8500-98-014 issued by USRA.
NR 36
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 OCT 20
PY 2014
VL 794
IS 2
AR 108
DI 10.1088/0004-637X/794/2/108
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8OF
UT WOS:000343085800012
ER

PT J
AU Nielsen, EL
   Liu, MC
   Wahhaj, Z
   Biller, BA
   Hayward, TL
   Males, JR
   Close, LM
   Morzinski, KM
   Skemer, AJ
   Kuchner, MJ
   Rodigas, TJ
   Hinz, PM
   Chun, M
   Ftaclas, C
   Toomey, DW
AF Nielsen, Eric L.
   Liu, Michael C.
   Wahhaj, Zahed
   Biller, Beth A.
   Hayward, Thomas L.
   Males, Jared R.
   Close, Laird M.
   Morzinski, Katie M.
   Skemer, Andrew J.
   Kuchner, Marc J.
   Rodigas, Timothy J.
   Hinz, Philip M.
   Chun, Mark
   Ftaclas, Christ
   Toomey, Douglas W.
TI THE GEMINI NICI PLANET-FINDING CAMPAIGN: THE ORBIT OF THE YOUNG
   EXOPLANET beta PICTORIS b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planet-disk interactions; planets and satellites:
   detection; stars: individual (beta Pic)
ID DEBRIS DISK; EXTRASOLAR PLANETS; GIANT PLANET; MOVING GROUP;
   ECCENTRICITY DISTRIBUTION; NEAR-IR; STARS; DISCOVERY; FREQUENCY;
   COMPANION
AB We present new astrometry for the young (12-21 Myr) exoplanet beta Pictoris b taken with the Gemini/NICI and Magellan/MagAO instruments between 2009 and 2012. The high dynamic range of our observations allows us to measure the relative position of beta Pic b with respect to its primary star with greater accuracy than previous observations. Based on a Markov Chain Monte Carlo analysis, we find the planet has an orbital semi-major axis of 9.1(-0.5)(+5.3) AU and orbital eccentricity <0.15 at 68% confidence (with 95% confidence intervals of 8.2-48 AU and 0.00-0.82 for semi-major axis and eccentricity, respectively, due to a long narrow degenerate tail between the two). We find that the planet has reached its maximum projected elongation, enabling higher precision determination of the orbital parameters than previously possible, and that the planet's projected separation is currently decreasing. With unsaturated data of the entire beta Pic system (primary star, planet, and disk) obtained thanks to NICI's semi-transparent focal plane mask, we are able to tightly constrain the relative orientation of the circumstellar components. We find the orbital plane of the planet lies between the inner and outer disks: the position angle (P.A.) of nodes for the planet's orbit (211.8 +/- 0 degrees.3) is 7.4 sigma greater than the P. A. of the spine of the outer disk and 3.2 sigma less than the warped inner disk P. A., indicating the disk is not collisionally relaxed. Finally, for the first time we are able to dynamically constrain the mass of the primary star beta Pic to 1.76(-0.17)(+0.18) M-circle dot.
C1 [Nielsen, Eric L.; Liu, Michael C.; Chun, Mark; Ftaclas, Christ] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
   [Wahhaj, Zahed] European So Observ, Santiago 19001, Chile.
   [Biller, Beth A.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
   [Hayward, Thomas L.] AURA, Southern Operat Ctr, Gemini Observ, La Serena, Chile.
   [Males, Jared R.; Close, Laird M.; Morzinski, Katie M.; Skemer, Andrew J.; Hinz, Philip M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
   [Kuchner, Marc J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Rodigas, Timothy J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
   [Toomey, Douglas W.] Mauna Kea Infrared LLC, Hilo, HI 96720 USA.
RP Nielsen, EL (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
OI Nielsen, Eric/0000-0001-6975-9056
FU Hubble Fellowship grant [HST-HF-01204.01-A]; NASA [NAS 5-26555]; NSF
   [AST-0713881, AST-0709484]; NASA Origins of Solar Systems; Space
   Telescope Science Institute
FX We thank Jessica Lu and Adam Kraus for helpful discussions. B.A.B. was
   supported in part by Hubble Fellowship grant HST-HF-01204.01-A awarded
   by the Space Telescope Science Institute, which is operated by AURA for
   NASA under contract NAS 5-26555. This work was supported in part by NSF
   grants AST-0713881 and AST-0709484 awarded to M. Liu. The MagAO portion
   of this work is supported, in part, by the NASA Origins of Solar Systems
   (PI: L. Close). The Gemini Observatory is operated by the Association of
   Universities for Research in Astronomy, Inc., under a cooperative
   agreement with the NSF on behalf of the Gemini partnership: the National
   Science Foundation (United States), the Science and Technology
   Facilities Council (United Kingdom), the National Research Council
   (Canada), CONICYT (Chile), the Australian Research Council (Australia),
   CNPq (Brazil), and CONICET (Argentina). This research has made use of
   the SIMBAD database, operated at CDS, Strasbourg, France.
NR 47
TC 17
Z9 17
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 OCT 20
PY 2014
VL 794
IS 2
AR 158
DI 10.1088/0004-637X/794/2/158
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8OF
UT WOS:000343085800062
ER

PT J
AU Sheets, HA
   Deming, D
AF Sheets, Holly A.
   Deming, Drake
TI STATISTICAL ECLIPSES OF CLOSE-IN KEPLER SUB-SATURNS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; occultations; planetary systems; planets and
   satellites: atmospheres; planets and satellites: surfaces; techniques:
   photometric
ID SUPER-EARTH ATMOSPHERES; HOT JUPITERS; LIGHT CURVES; ERROR-CORRECTION;
   INPUT CATALOG; PLANET; CANDIDATES; EXOPLANETS; ALBEDO; MODEL
AB We present a method to detect small atmospheric signals in Kepler's planet candidate light curves by averaging light curves for multiple candidates with similar orbital and physical characteristics. Our statistical method allows us to measure unbiased physical properties of Kepler's planet candidates, even for candidates whose individual signal-to- noise precludes the detection of their secondary eclipse. We detect a secondary eclipse depth of 3.83(-1.11)(+1.10) ppm for a group of 31 sub-Saturn (R < 6 R-circle plus) planet candidates with the greatest potential for a reflected light signature ((R-p/a)(2) > 10 ppm). Including Kepler-10b in this group increases the depth to 5.08(-0.72)(+0.71) ppm. For a control group with (R-p/a)(2) < 1 ppm, we find a depth of 0.36 +/- 0.37 ppm, consistent with no detection. We also analyze the light curve of Kepler-10b and find an eclipse depth of 7.08 +/- 1.06 ppm. If the eclipses are due solely to reflected light, this corresponds to a geometric albedo of 0.22 +/- 0.06 for our group of close-in sub-Saturns, 0.37 +/- 0.05 if including Kepler-10b in the group, and 0.60 +/- 0.09 for Kepler-10b alone. Including a thermal emission model does not change the geometric albedo appreciably, assuming A(B) = (3/2) * A(g). Our result for Kepler-10b is consistent with previous works. Our result for close-in sub-Saturns shows that Kepler-10b is unusually reflective, but our analysis is consistent with the results of Demory for super-Earths. Our results also indicate that hot Neptunes are typically more reflective than hot Jupiters.
C1 [Sheets, Holly A.; Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Sheets, Holly A.; Deming, Drake] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA.
RP Sheets, HA (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM hsheets@astro.umd.edu
FU NASA Science Mission directorate; NASA [NAS5-26555]; NASA Office of
   Space Science [NNX13AC07G]
FX We would like to thank the referee for comments and suggestions which
   helped to improve this work. This paper includes data collected by the
   Kepler mission. Funding for the Kepler mission is provided by the NASA
   Science Mission directorate. All 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-Hubble Space Telescope 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.
NR 42
TC 10
Z9 10
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 OCT 20
PY 2014
VL 794
IS 2
AR 133
DI 10.1088/0004-637X/794/2/133
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8OF
UT WOS:000343085800037
ER

PT J
AU Stern, D
   Lansbury, GB
   Assef, RJ
   Brandt, WN
   Alexander, DM
   Ballantyne, DR
   Balokovic, M
   Bauer, FE
   Benford, D
   Blain, A
   Boggs, SE
   Bridge, C
   Brightman, M
   Christensen, FE
   Comastri, A
   Craig, WW
   Del Moro, A
   Eisenhardt, PRM
   Gandhi, P
   Griffith, RL
   Hailey, CJ
   Harrison, FA
   Hickox, RC
   Jarrett, TH
   Koss, M
   Lake, S
   LaMassa, SM
   Luo, B
   Tsai, CW
   Urry, CM
   Walton, DJ
   Wright, EL
   Wu, J
   Yan, L
   Zhang, WW
AF Stern, D.
   Lansbury, G. B.
   Assef, R. J.
   Brandt, W. N.
   Alexander, D. M.
   Ballantyne, D. R.
   Balokovic, M.
   Bauer, F. E.
   Benford, D.
   Blain, A.
   Boggs, S. E.
   Bridge, C.
   Brightman, M.
   Christensen, F. E.
   Comastri, A.
   Craig, W. W.
   Del Moro, A.
   Eisenhardt, P. R. M.
   Gandhi, P.
   Griffith, R. L.
   Hailey, C. J.
   Harrison, F. A.
   Hickox, R. C.
   Jarrett, T. H.
   Koss, M.
   Lake, S.
   LaMassa, S. M.
   Luo, B.
   Tsai, C. -W.
   Urry, C. M.
   Walton, D. J.
   Wright, E. L.
   Wu, J.
   Yan, L.
   Zhang, W. W.
TI NuSTAR AND XMM-NEWTON OBSERVATIONS OF LUMINOUS, HEAVILY OBSCURED,
   WISE-SELECTED QUASARS AT Z similar to 2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; quasars: individual (WISEA J181417.29+341224.8, WISEA
   J220743.82+193940.1, WISEA J235710.82+032802
ID ACTIVE GALACTIC NUCLEI; RESOLUTION SPECTRAL TEMPLATES; SUPERMASSIVE
   BLACK-HOLES; PHOTON IMAGING CAMERA; DIGITAL SKY SURVEY; LY-ALPHA
   EMISSION; X-RAY LUMINOSITY; MIDINFRARED SELECTION; REDSHIFT
   Z-SIMILAR-TO-2; EXTRAGALACTIC SURVEY
AB We report on a NuSTAR and XMM-Newton program that has observed a sample of three extremely luminous, heavily obscured WISE-selected active galactic nuclei (AGNs) at z similar to 2 across a broad X-ray band (0.1 -79 keV). The parent sample, selected to be faint or undetected in the WISE 3.4 mu m (W1) and 4.6 mu m (W2) bands but bright at 12 mu m (W3) and 22 mu m (W4), are extremely rare, with only similar to 1000 so-called "W1W2-dropouts" across the extragalactic sky. Optical spectroscopy reveals typical redshifts of z similar to 2 for this population, implying rest-frame mid-IR luminosities of nu L-nu (6 mu m) similar to 6 x 10(46) erg s(-1) and bolometric luminosities that can exceed L-bol similar to 10(14) L-circle dot. The corresponding intrinsic, unobscured hard X-ray luminosities are L(2-10 keV) similar to 4 x 10(45) erg s-(1) for typical quasar templates. These are among the most AGNs known, though the optical spectra rarely show evidence of a broad-line region and the selection criteria imply heavy obscuration even at rest-frame 1.5mm. We designed our X-ray observations to obtain robust detections for gas column densities N-H <= 10(24) cm(-2). In fact, the sources prove to be fainter than these predictions. Two of the sources were observed by both NuSTAR and XMM-Newton, with neither being detected by NuSTAR (f(3-24 keV) less than or similar to 10(-13) erg cm(-2) s(-1)), and one being faintly detected by XMM-Newton (f(0.5-10 keV) similar to 5 x 10(-15) erg cm(-2) s(-1)). A third source was observed only with XMM-Newton, yielding a faint detection (f(0.5-10 keV) similar to 7 x 10(-15) erg cm(-2) s(-1)). The X-ray data imply these sources are either X-ray weak, or are heavily obscured by column densities N-H greater than or similar to 10(24) cm(-2). The combined X-ray and mid-IR analysis seems to favor this second possibility, implying the sources are extremely obscured, consistent with Compton-thick, luminous quasars. The discovery of a significant population of heavily obscured, extremely luminous AGNs would not conform to the standard paradigm of a receding torus, in which more luminous quasars are less likely to be obscured, and instead suggests that an additional source of obscuration is present in these extreme sources.
C1 [Stern, D.; Eisenhardt, P. R. M.; Tsai, C. -W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Lansbury, G. B.; Alexander, D. M.; Del Moro, A.; Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
   [Assef, R. J.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile.
   [Brandt, W. N.; Griffith, R. L.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
   [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
   [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
   [Balokovic, M.; Bridge, C.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
   [Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
   [Bauer, F. E.] Millennium Inst Astrophys, Santiago 7820436, Chile.
   [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
   [Benford, D.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Blain, A.] Univ Leicester, Leicester LE1 7RH, Leics, England.
   [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Brightman, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
   [Christensen, F. E.] Danish Tech Univ, DK-2800 Lyngby, Denmark.
   [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.
   [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
   [Jarrett, T. H.] Univ Cape Town, Dept Astron, Astrophys Cosmol & Grav Ctr, ZA-7700 Rondebosch, South Africa.
   [Koss, M.] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
   [Lake, S.; Wright, E. L.; Wu, J.] Univ Calif Los Angeles, Div Astron & Astrophys, Los Angeles, CA 90095 USA.
   [LaMassa, S. M.; Urry, C. M.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
   [LaMassa, S. M.; Urry, C. M.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
   [Yan, L.] CALTECH, Ctr Infrared Proc & Anal, Dept Astron, Pasadena, CA 91125 USA.
RP Stern, D (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 169-221, Pasadena, CA 91109 USA.
EM daniel.k.stern@jpl.nasa.gov
RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt,
   William/N-2844-2015; Comastri, Andrea/O-9543-2015; Benford,
   Dominic/D-4760-2012; 
OI Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581;
   Brandt, William/0000-0002-0167-2453; Comastri,
   Andrea/0000-0003-3451-9970; Benford, Dominic/0000-0002-9884-4206; Urry,
   Meg/0000-0002-0745-9792
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
   Science and Technology Facilities Council (STFC) [ST/K501979/1,
   ST/I001573/1, ST/J003697/1]; Leverhulme Trust; Gemini-CONICYT
   [32120009]; CONICYT-Chile [Basal-CATA PFB-06/2007, FONDECYT 1141218,
   "EMBIGGEN" Anillo ACT1101]; Project IC120009 "Millennium Institute of
   Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de
   Economia, Fomento y Turismo; ASI-INAF [I/37/012/0-011/13]; NASA through
   ADAP [NNX12AE38G]; National Science Foundation [1211096]; Swiss National
   Science Foundation (NSF) [PP00P2 138979/1]
FX We gratefully acknowledge the suggestions made by the anonymous referee,
   which have improved this manuscript. This work was supported under NASA
   Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a
   project led by the California Institute of Technology, managed by the
   Jet Propulsion Laboratory, and funded by the National Aeronautics and
   Space Administration. We thank the NuSTAR Operations, Software, and
   Calibration teams for support with the execution and analysis of these
   observations. This research has made use of the NuSTAR Data Analysis
   Software (NuSTARDAS) jointly developed by the ASI Science Data Center
   (ASDC, Italy) and the California Institute of Technology (USA). This
   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. We acknowledge financial support from the Science and
   Technology Facilities Council (STFC) grants ST/K501979/1 (G.B.L.),
   ST/I001573/1 (D.M.A. and A.D.M.), and ST/J003697/1 (P.G.), and the
   Leverhulme Trust (D.M.A. and J.R.M.). R.J.A. was supported by
   Gemini-CONICYT grant number 32120009. F.E.B. acknowledges support from
   CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, and "EMBIGGEN"
   Anillo ACT1101) and Project IC120009 "Millennium Institute of
   Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de
   Economia, Fomento y Turismo. A.C. acknowledges support from ASI-INAF
   grant I/37/012/0-011/13. R.C.H. acknowledges support from NASA through
   ADAP award NNX12AE38G and the National Science Foundation through grant
   number 1211096. M.K. acknowledges support from Swiss National Science
   Foundation (NSF) grant PP00P2 138979/1.
NR 64
TC 38
Z9 38
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 OCT 20
PY 2014
VL 794
IS 2
AR 102
DI 10.1088/0004-637X/794/2/102
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8OF
UT WOS:000343085800006
ER

PT J
AU Potter, C
AF Potter, Christopher
TI Ten years of forest cover change in the Sierra Nevada detected using
   Landsat satellite image analysis
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID MIXED-CONIFER FOREST; THEMATIC MAPPER DATA; POSTFIRE VEGETATION;
   ANCILLARY DATA; FIRE; CALIFORNIA; DISTURBANCE; CLIMATE; TM; RECOVERY
AB The Sierra Nevada of California is a region where large wildfires have been suppressed for over a century. A detailed geographic record of recent vegetation regrowth and disturbance patterns in forests of the Sierra Nevada remains a gap that can be filled with remote-sensing data. Landsat Thematic Mapper imagery was analysed to detect 10years of recent changes (between 2000 and 2009) in forest vegetation cover for areas burned by wildfires between years of 1995 and 1999 in the region. Results confirmed the prevalence of regrowing forest vegetation during the period 2000 and 2009 over 17% of the combined burned areas. Classification of these regrowing forest vegetation areas by the Landsat normalized burn ratio (NBR) showed that there was a marked increase in average disturbance index (Delta DI) values in the transitions from low to moderate to high burn severity classes. Within the five combined wildfire perimeters, 45% of the high burn severity area delineated by the RdNBR analysis was covered by regrowing forest detected between 2000 and 2009. In contrast, a notable fraction (12%) of the entire 5 km (unburned) buffer area outside the 1995-1999 fires perimeters showed decline in forest cover, and not nearly as many regrowing forest areas, covering only 3% of all the 1995-1999 buffer areas combined. Based on comparison of these results to ground-based survey data and high-resolution aerial images, the Landsat difference index (Delta DI) methodology can fulfil much of the need for consistent, low-cost monitoring of changes due to climate and biological factors in western forest regrowth following stand-replacing disturbances.
C1 NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Potter, C (reprint author), NASA Ames Res Ctr, Mail Stop 232-21, Moffett Field, CA 94035 USA.
EM chris.potter@nasa.gov
NR 49
TC 3
Z9 3
U1 5
U2 25
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0143-1161
EI 1366-5901
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PD OCT 18
PY 2014
VL 35
IS 20
BP 7136
EP 7153
DI 10.1080/01431161.2014.968687
PG 18
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA AR8EM
UT WOS:000343808500003
ER

PT J
AU Turner, W
AF Turner, Woody
TI Sensing biodiversity
SO SCIENCE
LA English
DT Editorial Material
C1 NASA Headquarters, Div Earth Sci, Washington, DC 20546 USA.
RP Turner, W (reprint author), NASA Headquarters, Div Earth Sci, Washington, DC 20546 USA.
EM woody.turner@nasa.gov
NR 14
TC 20
Z9 21
U1 5
U2 69
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 OCT 17
PY 2014
VL 346
IS 6207
BP 301
EP 302
DI 10.1126/science.1256014
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AQ7ZY
UT WOS:000343041100018
PM 25324372
ER

PT J
AU Peter, H
   Tian, H
   Curdt, W
   Schmit, D
   Innes, D
   De Pontieu, B
   Lemen, J
   Title, A
   Boerner, P
   Hurlburt, N
   Tarbell, TD
   Wuelser, JP
   Martinez-Sykora, J
   Kleint, L
   Golub, L
   McKillop, S
   Reeves, KK
   Saar, S
   Testa, P
   Kankelborg, C
   Jaeggli, S
   Carlsson, M
   Hansteen, V
AF Peter, H.
   Tian, H.
   Curdt, W.
   Schmit, D.
   Innes, D.
   De Pontieu, B.
   Lemen, J.
   Title, A.
   Boerner, P.
   Hurlburt, N.
   Tarbell, T. D.
   Wuelser, J. P.
   Martinez-Sykora, Juan
   Kleint, L.
   Golub, L.
   McKillop, S.
   Reeves, K. K.
   Saar, S.
   Testa, P.
   Kankelborg, C.
   Jaeggli, S.
   Carlsson, M.
   Hansteen, V.
TI Hot explosions in the cool atmosphere of the Sun
SO SCIENCE
LA English
DT Article
ID ELLERMAN BOMBS; H-ALPHA; SOLAR; FLUX; EMERGENCE; REGION; CHROMOSPHERE;
   CONVECTION
AB The solar atmosphere was traditionally represented with a simple one-dimensional model. Over the past few decades, this paradigm shifted for the chromosphere and corona that constitute the outer atmosphere, which is now considered a dynamic structured envelope. Recent observations by the Interface Region Imaging Spectrograph (IRIS) reveal that it is difficult to determine what is up and down, even in the cool 6000-kelvin photosphere just above the solar surface: This region hosts pockets of hot plasma transiently heated to almost 100,000 kelvin. The energy to heat and accelerate the plasma requires a considerable fraction of the energy from flares, the largest solar disruptions. These IRIS observations not only confirm that the photosphere is more complex than conventionally thought, but also provide insight into the energy conversion in the process of magnetic reconnection.
C1 [Peter, H.; Curdt, W.; Schmit, D.; Innes, D.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
   [Tian, H.; Golub, L.; McKillop, S.; Reeves, K. K.; Saar, S.; Testa, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [De Pontieu, B.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.; Martinez-Sykora, Juan; Kleint, L.] LMSAL, Palo Alto, CA 94304 USA.
   [Martinez-Sykora, Juan; Kleint, L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
   [Kleint, L.] NASA, Ames Res Ctr, Moffett Field, CA 94305 USA.
   [Kankelborg, C.; Jaeggli, S.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
   [De Pontieu, B.; Carlsson, M.; Hansteen, V.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway.
RP Peter, H (reprint author), Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
EM peter@mps.mpg.de
RI Reeves, Katharine/P-9163-2014
FU Norwegian Space Centre through European Space Agency PRODEX; NASA
   [NNG09FA40C, NNX11AO98G]; Lockheed Martin Independent Research Program;
   European Research Council [291058]
FX H.P. thanks LMSAL for hospitality during his visit. We thank R. Rutten
   for countless comments and good discussions and two anonymous referees
   for valuable comments. IRIS is a NASA Small Explorer mission developed
   and operated by LMSAL, with mission, operations executed at NASA Ames
   Research Center and major contributions to downlink communications
   funded by the Norwegian Space Centre through a European Space Agency
   PRODEX contract. This work is supported by NASA contract NNG09FA40C
   (IRIS), the Lockheed Martin Independent Research Program, European
   Research Council grant agreement 291058, and NASA grant NNX11AO98G. The
   Solar Dynamics Observatory (SDO) data that we used are provided courtesy
   of NASA/SDO and the Atmospheric Imaging Assembly and Helioseismic and
   Magnetic Imager science teams. All data used in this study are publicly
   available through the Virtual Solar Observatory
   (http://sdac.virtualsolar.org). The IRIS data are archived at
   http://iris.lmsal.com/data.html, where manuals for data reduction are
   also available.
NR 27
TC 47
Z9 48
U1 1
U2 11
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD OCT 17
PY 2014
VL 346
IS 6207
AR 1255726
DI 10.1126/science.1255726
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AQ7ZY
UT WOS:000343041100033
PM 25324397
ER

PT J
AU Testa, P
   De Pontieu, B
   Allred, J
   Carlsson, M
   Reale, F
   Daw, A
   Hansteen, V
   Martinez-Sykora, J
   Liu, W
   DeLuca, EE
   Golub, L
   McKillop, S
   Reeves, K
   Saar, S
   Tian, H
   Lemen, J
   Title, A
   Boerner, P
   Hurlburt, N
   Tarbell, TD
   Wuelser, JP
   Kleint, L
   Kankelborg, C
   Jaeggli, S
AF Testa, P.
   De Pontieu, B.
   Allred, J.
   Carlsson, M.
   Reale, F.
   Daw, A.
   Hansteen, V.
   Martinez-Sykora, J.
   Liu, W.
   DeLuca, E. E.
   Golub, L.
   McKillop, S.
   Reeves, K.
   Saar, S.
   Tian, H.
   Lemen, J.
   Title, A.
   Boerner, P.
   Hurlburt, N.
   Tarbell, T. D.
   Wuelser, J. P.
   Kleint, L.
   Kankelborg, C.
   Jaeggli, S.
TI Evidence of nonthermal particles in coronal loops heated impulsively by
   nanoflares
SO SCIENCE
LA English
DT Article
ID X-RAY OBSERVATIONS; SOLAR-FLARES; FREQUENCY-DISTRIBUTIONS; ELECTRON
   ACCELERATION; WAVES; CHROMOSPHERE; PROPAGATION; STATISTICS; EMISSION;
   PLASMA
AB The physical processes causing energy exchange between the Sun's hot corona and its cool lower atmosphere remain poorly understood. The chromosphere and transition region (TR) form an interface region between the surface and the corona that is highly sensitive to the coronal heating mechanism. High-resolution observations with the Interface Region Imaging Spectrograph (IRIS) reveal rapid variability (similar to 20 to 60 seconds) of intensity and velocity on small spatial scales (less than or similar to 500 kilometers) at the footpoints of hot and dynamic coronal loops. The observations are consistent with numerical simulations of heating by beams of nonthermal electrons, which are generated in small impulsive (less than or similar to 30 seconds) heating events called "coronal nanoflares." The accelerated electrons deposit a sizable fraction of their energy (less than or similar to 10(25) erg) in the chromosphere and TR. Our analysis provides tight constraints on the properties of such electron beams and new diagnostics for their presence in the nonflaring corona.
C1 [Testa, P.; DeLuca, E. E.; Golub, L.; McKillop, S.; Reeves, K.; Saar, S.; Tian, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [De Pontieu, B.; Liu, W.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.; Kleint, L.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
   [De Pontieu, B.; Carlsson, M.; Hansteen, V.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
   [Allred, J.; Daw, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Reale, F.] Univ Palermo, Dipartimento Fis & Chim, I-90134 Palermo, Italy.
   [Reale, F.] Ist Nazl Astrofis INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy.
   [Martinez-Sykora, J.; Kleint, L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
   [Liu, W.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
   [Kankelborg, C.; Jaeggli, S.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
RP Testa, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ptesta@cfa.harvard.edu
RI Reeves, Katharine/P-9163-2014; 
OI Reale, Fabio/0000-0002-1820-4824
FU Norwegian Space Center (NSC, Norway) through European Space Agency
   PRODEX; NASA [NNG09FA40C, NNX13AF79G]; Lockheed Martin Independent
   Research Program; European Research Council from Lockheed-Martin
   [291058, 8100002705]; Research Council of Norway
FX IRIS is a NASA Small Explorer mission, developed and operated by
   Lockheed Martin Solar and Astrophysics Laboratory 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 European Space Agency PRODEX contract. The IRIS data
   can be accessed at http://iris.lmsal.com/search/, and the AIA data at
   www.lmsal.com/get_aia_data/. This work is supported by NASA under
   contract NNG09FA40C (IRIS) and the Lockheed Martin Independent Research
   Program, the European Research Council grant agreement no.291058, and
   contract 8100002705 from Lockheed-Martin to the Smithsonian
   Astrophysical Observatory. M.C. acknowledges funding from the Research
   Council of Norway. W.L. is supported by NASA Living with a Star-Targeted
   Research and Technology grant NNX13AF79G.
NR 30
TC 37
Z9 37
U1 4
U2 17
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 OCT 17
PY 2014
VL 346
IS 6207
AR 1255724
DI 10.1126/science.1255724
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AQ7ZY
UT WOS:000343041100032
PM 25324396
ER

PT J
AU Liou, K
   Sibeck, DG
AF Liou, Kan
   Sibeck, David G.
TI Study of a global auroral Pc5 pulsation event with concurrent ULF waves
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID FIELD-LINE RESONANCES; MAGNETOSPHERE; OSCILLATIONS; INSTABILITIES;
   SUBSTORM; MIRROR; CAVITY; ORBIT
AB We present results from a study of concurrent, periodic variations in auroral luminosity (auroral pulsations) and in magnetospheric plasma/magnetic field data. This event occurred on 10 March 2010 from similar to 13 to 17 UT during an extended southward interplanetary magnetic field and was probably triggered by a slow shock. The auroral pulsations, as measured by the Ultraviolet Imager on board the Polar satellite, were long lasting (similar to 2.5 h), monochromatic (similar to 2.5mHz), large scale, and appeared in the night sector auroral zone with a latitudinal extent comparable to the latitudinal width of the oval. There was no phase shift between the auroral pulsations observed at different local times, indicating a stationary structure. Particle data from the Defense Meteorological Satellite Program Special Sensor Precipitating Electron and Ion Spectrometer indicate that the pulsations were diffuse originating from the central plasma sheet. During this time, Geotail was in the dawn sector plasma sheet and observed a ULF wave with the same frequency as the auroral pulsations last similar to 35 min. The ULF wave had large radial and compressional components, and the plasma density and total magnetic field were anticorrelated. These two observations strongly suggest that the observed ULF wave was associated with an standing ULF poloidal mode. The wave compressional component may be able to change the loss cone, resulting in periodic auroral precipitating.
C1 [Liou, Kan] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
   [Sibeck, David G.] NASA GSFC, Greenbelt, MD USA.
RP Liou, K (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
EM kan.liou@jhuap.edu
RI Liou, Kan/C-2089-2016
OI Liou, Kan/0000-0001-5277-7688
FU NSF grant [AGS-0964396]
FX We acknowledge the use of the NASA/GSFC's Space Physics Data Facility's
   OMNIWeb (or CDAWeb or ftp) service and OMNI data. G.K. Parks was the PI
   for the Polar UVI, which was built by M. Torr. The Geotail IMF data were
   provided by S. Kokubun (PI of MGF) through DARTS, and the Geotail solar
   wind data were courtesy of T. Mukai (PI of LEP). JHUAPL provided the
   DMSP particle spectrograms, which are made possible by P.T. Newell and
   T. Sotirelis. The DMSP SSJ/4 particle detectors were designed and
   calibrated by Dave Hardy, Fred Rich, and colleagues at AFRL at Hanscom
   AFB in Boston. The U.S. Air Force has publicly released these data. Most
   of it was obtained through WDC-A (NOAA) in Boulder, with generous
   supplements from AFRL. This work was supported by the NSF grant
   AGS-0964396 to the Johns Hopkins University Applied Physics Laboratory.
NR 41
TC 2
Z9 3
U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 16
PY 2014
VL 41
IS 19
BP 6547
EP 6555
DI 10.1002/2014GL060755
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA AT4MP
UT WOS:000344913800001
ER

PT J
AU Murphy, KR
   Mann, IR
   Ozeke, LG
AF Murphy, Kyle R.
   Mann, Ian R.
   Ozeke, Louis G.
TI A ULF wave driver of ring current energization
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID RELATIVISTIC ELECTRON FLUX; SOLAR-WIND SPEED; RADIATION; ACCELERATION;
   MODEL; FIELD; POWER; MAGNETOSPHERE; DEPENDENCE; INJECTION
AB ULF wave radial diffusion plays an important role in the transport of energetic electrons in the outer radiation belt, yet similar ring current transport is seldom considered even though ions satisfy a nearly identical drift resonance condition albeit without the relativistic correction. By examining the correlation between ULF wave power and the response of the ring current, characterized by Dst, we demonstrate a definite correlation between ULF wave power and Dst. Significantly, the lagged correlation peaks such that ULF waves precede the response of the ring current and Dst. We suggest that this correlation is the result of enhanced radial transport and energization of ring current ions through drift resonance and ULF wave radial diffusion of ring current ions. An analysis and comparison of the ion and electron diffusion coefficients further support this conclusion, ULF waves providing an important missing physical transport process explaining Dst underestimation in ring current models.
C1 [Murphy, Kyle R.] NASA GSFC, Greenbelt, MD 20771 USA.
   [Murphy, Kyle R.; Mann, Ian R.; Ozeke, Louis G.] Univ Alberta, Dept Phys, Edmonton, AB, Canada.
RP Murphy, KR (reprint author), NASA GSFC, Greenbelt, MD 20771 USA.
EM kyle.r.murphy@nasa.gov
FU NSERC Postdoctoral Fellowship; Discovery grant from Canadian NSERC;
   Canadian Space Agency; European Community [284520]; NASA THEMIS mission;
   NASA Van Allen Probes mission
FX K.R.M. is funded by an NSERC Postdoctoral Fellowship. I.R.M. is
   supported by a Discovery grant from Canadian NSERC. Magnetometer data
   were provided by the CARISMA magnetometer array and can be downloaded at
   www.carisma.ca. We thank D.K. Milling and the rest of the CARISMA team
   for the data. CARISMA is operated by the University of Alberta and
   funded by the Canadian Space Agency. The Sub-Auroral Magnetometer
   Network data (SAMNET) are operated by the Space Plasma Environment and
   Radio Science (SPEARS) group, Department of Physics, Lancaster
   University. The Dst index was provided by OmniWeb at
   omniweb.gsfc.nasa.gov. This work was supported in part by participation
   in the MAARBLE (Monitoring, Analyzing and Assessing Radiation Belt Loss
   and Energization) consortium. MAARBLE has received funding from the
   European Community's Seventh Framework Programme (FP7-SPACE-2010-1, SP1
   Cooperation, Collaborative project) under grant agreement 284520. This
   paper reflects only the authors' views, and the European Union is not
   liable for any use that may be made of the information contained herein.
   This work was partially funded by the NASA THEMIS and Van Allen Probes
   missions.
NR 37
TC 2
Z9 2
U1 0
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 OCT 16
PY 2014
VL 41
IS 19
BP 6595
EP 6602
DI 10.1002/2014GL061253
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AT4MP
UT WOS:000344913800008
ER

PT J
AU Philpott, LC
   Johnson, CL
   Winslow, RM
   Anderson, BJ
   Korth, H
   Purucker, ME
   Solomon, SC
AF Philpott, Lydia C.
   Johnson, Catherine L.
   Winslow, Reka M.
   Anderson, Brian J.
   Korth, Haje
   Purucker, Michael E.
   Solomon, Sean C.
TI Constraints on the secular variation of Mercury's magnetic field from
   the combined analysis of MESSENGER and Mariner 10 data
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID CRUSTAL REMANENCE; MAGNETOPAUSE; GENERATION
AB Observations of Mercury's internal magnetic field from the Magnetometer on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft have revealed a dipole moment of 190 nT R-M(3) offset about 480 km northward from the planetary equator, where R-M is Mercury's radius. We have reanalyzed magnetic field observations acquired by the Mariner 10 spacecraft during its third flyby of Mercury (M10-III) in 1975 to constrain the secular variation in the internal field over the past 40 years. With the application of techniques developed in the analysis of MESSENGER data, we find that the dipole moment that best fits the M10-III data is 188 nT R-M(3) offset 475 km northward from the equator. Our results are consistent with no secular variation, although variations of up to 10%, 16%, and 35%, respectively, are permitted in the zonal coefficients g(1)(0), g(2)(0), and g(3)(0) in a spherical harmonic expansion of the internal field.
C1 [Philpott, Lydia C.; Johnson, Catherine L.; Winslow, Reka M.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V5Z 1M9, Canada.
   [Johnson, Catherine L.] Planetary Sci Inst, Tucson, AZ USA.
   [Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
   [Purucker, Michael E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
   [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
RP Philpott, LC (reprint author), Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V5Z 1M9, Canada.
EM lphilpott@eos.ubc.ca
OI Philpott, Lydia/0000-0002-5286-8528
FU Natural Sciences and Engineering Research Council of Canada; NASA
   Discovery Program [NAS5-97271]; MESSENGER Participating Scientist grant
   [NNX11AB84G]
FX The Mariner 10 magnetic field data were obtained from the Planetary Data
   System (PDS). LCP, CLJ, and RMW acknowledge support from the Natural
   Sciences and Engineering Research Council of Canada. The MESSENGER
   project is supported by the NASA Discovery Program under contracts
   NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory
   and NASW-00002 to the Carnegie Institution of Washington. CLJ
   acknowledges support from MESSENGER Participating Scientist grant
   NNX11AB84G. MESSENGER data are available from the PDS
   (https://pds.jpl.nasa.gov).
NR 31
TC 4
Z9 4
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 16
PY 2014
VL 41
IS 19
BP 6627
EP 6634
DI 10.1002/2014GL061401
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AT4MP
UT WOS:000344913800012
ER

PT J
AU Grima, C
   Blankenship, DD
   Young, DA
   Schroeder, DM
AF Grima, Cyril
   Blankenship, Donald D.
   Young, Duncan A.
   Schroeder, Dustin M.
TI Surface slope control on firn density at Thwaites Glacier, West
   Antarctica: Results from airborne radar sounding
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID AMUNDSEN SEA EMBAYMENT; SNOW ACCUMULATION; ICE-SHEET;
   MICROWAVE-FREQUENCIES; DIELECTRIC-PROPERTIES; VARIABILITY; MODEL;
   REFLECTIVITY; MARS; MHZ
AB We derive the surface density variations over Thwaites Glacier from a statistical analysis of airborne High-Capability Radar Sounder surface returns acquired in the 2004-2005 summer. We produce a 5 km gridded map with an estimated +/- 12.5 kg m(-3) accuracy. The background pattern of densities decreases inland from similar to 480 kg m(-3) to similar to 350 kg m(-3). A remarkable similar to 30 km wide vein-shaped anomaly of up to 570 kg m(-3) is located similar to 100 km from the coastline. Density anomalies correspond with surface slope breaks but are not necessarily coincident with smaller slopes. They could result from complex wind-driven snow redistribution and/or refreezing of former snowmelt. This inversion technique can significantly improve surface mass balance calculations to understanding of glacier dynamics at regional scales and is valuable to verify and improve Antarctic climate models. It is also a promising approach for future surface analysis of icy moons by planetary radars.
C1 [Grima, Cyril; Blankenship, Donald D.; Young, Duncan A.; Schroeder, Dustin M.] Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA.
   [Schroeder, Dustin M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Grima, C (reprint author), Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA.
EM cyril.grima@gmail.com
RI Young, Duncan/G-6256-2010; 
OI Young, Duncan/0000-0002-6866-8176; Grima, Cyril/0000-0001-7135-3055
FU G. Unger Vetlesen Foundation; NASA's Instrument Concepts for Europa
   Exploration grant [13-ICEE13-00018]; National Aeronautics and Space
   Administration
FX We thank Brooke Medley for sharing accumulation rate data and two
   reviewers whose comments improved the manuscript. The data will be made
   available through NSIDC's ADGC. This work was supported by the G. Unger
   Vetlesen Foundation and NASA's Instrument Concepts for Europa
   Exploration grant 13-ICEE13-00018. 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.
   This is UTIG contribution.
NR 58
TC 5
Z9 5
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 OCT 16
PY 2014
VL 41
IS 19
BP 6787
EP 6794
DI 10.1002/2014GL061635
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AT4MP
UT WOS:000344913800033
ER

PT J
AU Kort, EA
   Frankenberg, C
   Costigan, KR
   Lindenmaier, R
   Dubey, MK
   Wunch, D
AF Kort, Eric A.
   Frankenberg, Christian
   Costigan, Keeley R.
   Lindenmaier, Rodica
   Dubey, Manvendra K.
   Wunch, Debra
TI Four corners: The largest US methane anomaly viewed from space
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID COLUMN OBSERVING NETWORK; ATMOSPHERIC METHANE; NATURAL-GAS; EMISSIONS;
   NORTH; ATTRIBUTION
AB Methane (CH4) is a potent greenhouse gas and ozone precursor. Quantifying methane emissions is critical for projecting and mitigating changes to climate and air quality. Here we present CH4 observations made from space combined with Earth-based remote sensing column measurements. Results indicate the largest anomalous CH4 levels viewable from space over the conterminous U.S. are located at the Four Corners region in the Southwest U. S. Emissions exceeding inventory estimates, totaling 0.59 Tg CH4/yr [0.50-0.67; 2 sigma],are necessary to bring high-resolution simulations and observations into agreement. This underestimated source approaches 10% of the EPA estimate of total U.S. CH4 emissions from natural gas. The persistence of this CH4 signal from 2003 onward indicates that the source is likely from established gas, coal, and coalbed methane mining and processing. This work demonstrates that space-based observations can identify anomalous CH4 emission source regions and quantify their emissions with the use of a transport model.
C1 [Kort, Eric A.] Univ Michigan, Ann Arbor, MI 48109 USA.
   [Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Costigan, Keeley R.; Lindenmaier, Rodica; Dubey, Manvendra K.] Los Alamos Natl Lab, Los Alamos, NM USA.
   [Wunch, Debra] CALTECH, Dept Earth Sci & Engn, Pasadena, CA 91125 USA.
RP Kort, EA (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA.
EM eakort@umich.edu
RI Kort, Eric/F-9942-2012; Dubey, Manvendra/E-3949-2010; Frankenberg,
   Christian/A-2944-2013
OI Kort, Eric/0000-0003-4940-7541; Dubey, Manvendra/0000-0002-3492-790X;
   Frankenberg, Christian/0000-0002-0546-5857
FU NASA [NNX14AI87G]; LANL's Laboratory Directed Research and Development
   Program [20110081DR]; DOE ASR; CCRD; OSc; LANL TCCON FTS
FX E.A.K. thanks the W. M. Keck Institute for Space Studies. Portions of
   this work were supported by NASA under award NNX14AI87G. Four Corners
   monitoring and modeling was supported by LANL's Laboratory Directed
   Research and Development Program (20110081DR, PI M. K. D.) with funds
   from DOE ASR, CCRD, and OSc to acquire and set up the LANL TCCON FTS.
   The Four Corners TCCON data were obtained from the TCCON Data Archive,
   operated by the California Institute of Technology from the website at
   http://tccon.ipac.caltech.edu/. Simulations were carried out on High
   Performance Computing resources under a grant from the LANL
   Institutional Computing Program. Portions of this work were conducted at
   the Jet Propulsion Laboratory, California Institute of Technology, under
   a contract with the National Aeronautics and Space Administration. The
   authors thank Mike Gunson for comments on the manuscript.
NR 31
TC 36
Z9 36
U1 4
U2 51
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 OCT 16
PY 2014
VL 41
IS 19
BP 6898
EP 6903
DI 10.1002/2014GL061503
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA AT4MP
UT WOS:000344913800047
ER

PT J
AU Christensen, MW
   Suzuki, K
   Zambri, B
   Stephens, GL
AF Christensen, M. W.
   Suzuki, K.
   Zambri, B.
   Stephens, G. L.
TI Ship track observations of a reduced shortwave aerosol indirect effect
   in mixed-phase clouds
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID RADIATIVE-TRANSFER; STRATIFORM CLOUDS; ICE NUCLEATION; PARTICLES;
   EMISSIONS; PRECIPITATION; RETRIEVAL; SYSTEM; ALBEDO
AB Aerosol influences on clouds are a major source of uncertainty to our understanding of forced climate change. Increased aerosol can enhance solar reflection from clouds countering greenhouse gas warming. Recently, this indirect effect has been extended from water droplet clouds to other types including mixed-phase clouds. Aerosol effects on mixed-phase clouds are important because of their fundamental role on sea ice loss and polar climate change, but very little is known about aerosol effects on these clouds. Here we provide the first analysis of the effects of aerosol emitted from ship stacks into mixed-phase clouds. Satellite observations of solar reflection in numerous ship tracks reveal that cloud albedo increases 5 times more in liquid clouds when polluted and persist 2 h longer than in mixed-phase clouds. These results suggest that seeding mixed-phase clouds via shipping aerosol is unlikely to provide any significant counterbalancing solar radiative cooling effects in warming polar regions.
C1 [Christensen, M. W.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
   [Christensen, M. W.; Suzuki, K.; Stephens, G. L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Zambri, B.] Calif State Univ Northridge, Dept Math, Northridge, CA 91330 USA.
RP Christensen, MW (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
EM Matt.Christensen@jpl.nasa.gov
RI Suzuki, Kentaroh/C-3624-2011; Christensen, Matthew/C-5733-2013; 
OI Zambri, Brian/0000-0002-1497-1954
FU NASA's Innovations in Global Climate Change Education; CSU under NASA
   [NAS5-99237]; NASA [NNN13D771T]; JPL CloudSat [1439268]
FX We would like to thank the three anonymous reviewers for their detailed
   and insightful comments. We also thank the NASA Goddard (MODIS), the
   Cooperative Institute for Research in the Atmosphere (CloudSat), and the
   NASA Langley Research Center (CALIOP) distribution centers for providing
   the data used in this paper. We thank Jim Coakley of Oregon State
   University, for his explanations of the intricacies of MODIS cloud
   retrievals and continued interest in this research. At the time this
   work was performed, Brian Zambri was a summer intern at JPL through the
   California State University Northridge program "Mathematical and
   Geospatial Pathways to Climate Change Education" supported by NASA's
   Innovations in Global Climate Change Education. Part of the research was
   carried out at CSU under NASA grant NAS5-99237, the other portion at
   JPL, Caltech, under a contract with NASA funded by grant NNN13D771T and
   JPL CloudSat Subcontract 1439268.
NR 37
TC 2
Z9 2
U1 4
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 OCT 16
PY 2014
VL 41
IS 19
BP 6970
EP 6977
DI 10.1002/2014GL061320
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA AT4MP
UT WOS:000344913800057
ER

PT J
AU Li, JLF
   Lee, WL
   Waliser, DE
   Stachnik, JP
   Fetzer, E
   Wong, S
   Yue, Q
AF Li, J. -L. F.
   Lee, W. -L.
   Waliser, D. E.
   Stachnik, Justin P.
   Fetzer, Eric
   Wong, Sun
   Yue, Qing
TI Characterizing tropical Pacific water vapor and radiative biases in
   CMIP5 GCMs: Observation-based analyses and a snow and radiation
   interaction sensitivity experiment
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ATMOSPHERIC INFRARED SOUNDER; SURFACE IRRADIANCES; IN-SITU; CLOUD;
   REANALYSIS; SATELLITE; MODEL; PRODUCTS; PRECIPITATION; CLIMATOLOGY
AB Significant systematic biases in the moisture fields within the tropical Pacific trade wind regions are found in the Coupled Model Intercomparison Project (CMIP3/CMIP5) against profile and total column water vapor (TotWV) estimates from the Atmospheric Infrared Sounder and TotWV from the Special Sensor Microwave/Imager. Positive moisture biases occur in conjunction with significant biases of eastward low-level moisture convergence north of the South Pacific Convergence Zone and south of the Intertropical Convergence Zone-the V-shaped regions. The excessive moisture there is associated with overestimates of reflected upward shortwave (RSUT), underestimates of outgoing longwave radiation (RLUT) at the top of atmosphere (TOA), and underestimates of downward shortwave flux at the surface (RSDS) compared to Clouds and the Earth's Energy System, Energy Balance and Filled data. We characterize the impacts of falling snow and its radiation interaction, which are not included in most CMIP5 models, on the moisture fields using the National Center for Atmospheric Research-coupled global climate model (GCM). A number of differences in the model simulation without snow-radiation interactions are consistent with biases in the CMIP5 simulations. These include effective low-level eastward/southeastward wind and surface wind stress anomalies, and an increase in TotWV, vertical profile of moisture, and cloud amounts in the V-shaped region. The anomalous water vapor and cloud amount might be associated with the model increase of RSUT and decrease of RLUT at TOA and decreased RSDS in clear and all sky in these regions. These findings hint at the importance of water vapor-radiation interactions in the CMIPS/CMIP5 model simulations that exclude the radiative effect of snow.
C1 [Li, J. -L. F.; Waliser, D. E.; Stachnik, Justin P.; Fetzer, Eric; Wong, Sun; Yue, Qing] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
   [Lee, W. -L.] Acad Sinica, RCEC, Taipei 115, Taiwan.
RP Li, JLF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Juilin.F.Li@jpl.nasa.gov
RI Stachnik, Justin/A-5609-2015; Yue, Qing/F-4619-2017
OI Yue, Qing/0000-0002-3559-6508
FU NNH12ZDA001N ROSES 2012; Earth Science Program; Modeling, Analysis, and
   Prediction (MAP); ATMOS COMP [NNH12ZDA001N-CCST]; NASA Making Earth
   System Data Records for Use in Research Environments (MEaSUREs);
   National Science Council [NSC100-2119-M-001-029-MY5,
   NSC102-2111-M-001-009]
FX We thank H.-H. Hsu at Academia Sinica, Taiwan, for useful comments and
   Bin Guan's help for data processing. The contributions by D. E. W. and
   J.L.L. to this study were carried out on behalf of the Jet Propulsion
   Laboratory, California Institute of Technology, under contracts of
   NNH12ZDA001N ROSES 2012, Earth Science Program, the Modeling, Analysis,
   and Prediction (MAP), and ATMOS COMP 2013 (NNH12ZDA001N-CCST) with the
   National Aeronautics and Space Administration (NASA). This work has been
   supported in part by the NASA Making Earth System Data Records for Use
   in Research Environments (MEaSUREs). W. L. L. was supported by National
   Science Council under contracts NSC100-2119-M-001-029-MY5 and
   NSC102-2111-M-001-009. Data supporting this study are available in Text
   S1 in the supporting information.
NR 45
TC 5
Z9 5
U1 2
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 16
PY 2014
VL 119
IS 19
BP 10981
EP 10995
DI 10.1002/2014JD021924
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS1PU
UT WOS:000344053400001
ER

PT J
AU Painemal, D
   Kato, S
   Minnis, P
AF Painemal, David
   Kato, Seiji
   Minnis, Patrick
TI Boundary layer regulation in the southeast Atlantic cloud microphysics
   during the biomass burning season as seen by the A-train satellite
   constellation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID VOCALS-REX; STRATOCUMULUS CLOUDS; MARINE STRATOCUMULUS; AERONET
   MEASUREMENTS; ABSORBING AEROSOLS; OPTICAL DEPTH; VARIABILITY; MODIS;
   PACIFIC; OCEAN
AB Solar radiation absorption by biomass burning aerosols has a strong warming effect over the southeast Atlantic. Interactions between the overlying smoke aerosols and low-level cloud microphysics and the subsequent albedo perturbation are, however, generally ignored in biomass burning radiative assessments. In this study, Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation (CALIPSO) are combined with Aqua satellite observations from Moderate Resolution Imaging Spectroradiometer (MODIS), Advanced Microwave Scanning Radiometer-EOS (AMSR-E), and Clouds and the Earth's Radiant Energy System (CERES) to assess the effect of variations in the boundary layer height and the separation distance between the cloud and aerosol layers on the cloud microphysics. The merged data analyzed at a daily temporal resolution suggest that overlying smoke aerosols modify cloud properties by decreasing cloud droplet size despite an increase in the cloud liquid water as boundary layer deepens, north of 5 degrees S. These changes are controlled by the proximity of the aerosol layer to the cloud top rather than increases in the column aerosol load. The correlations are unlikely driven by meteorological factors, as three predictors of cloud variability, lower tropospheric stability, surface winds, and mixing ratio suggest that cloud effective radius, cloud top height, and liquid water path should correlate positively. Because cloud effective radius anticorrelates with cloud liquid water over the region with large microphysical changes-north of 5 degrees S-the overall radiative consequence at the top of the atmosphere is a strong albedo susceptibility, equivalent to a 3% albedo increase due to a 10% decrease in cloud effective radius. This albedo enhancement partially offsets the aerosol solar absorption. Our analysis emphasizes the importance of accounting for the indirect effect of smoke aerosols in the cloud microphysics when estimating the radiative impact of the biomass burning at the top of the atmosphere.
C1 [Painemal, David; Kato, Seiji; Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
   [Painemal, David] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Painemal, D (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM david.painemal@nasa.gov
FU NASA-LaRC-NPP program; CERES project; NASA CERES; NEWS projects; MAP
   projects
FX D. Painemal was partially supported by the NASA-LaRC-NPP program and the
   CERES project. S. Kato was supported by the NASA CERES and NEWS
   projects. P. Minnis was supported by the NASA CERES and MAP projects.
   The AMSR-E retrievals were obtained at http://www.ssmi.com/. Figure 14
   was made using the interactive tool at
   http://www-calipso.larc.nasa.gov/products/lidar/browse_images/production
   /. The comments and suggestions of three anonymous reviewers are greatly
   acknowledged.
NR 61
TC 6
Z9 6
U1 1
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 16
PY 2014
VL 119
IS 19
BP 11288
EP 11302
DI 10.1002/2014JD022182
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS1PU
UT WOS:000344053400019
ER

PT J
AU Hu, XF
   Waller, LA
   Lyapustin, A
   Wang, YJ
   Liu, Y
AF Hu, Xuefei
   Waller, Lance A.
   Lyapustin, Alexei
   Wang, Yujie
   Liu, Yang
TI Improving satellite-driven PM2.5 models with Moderate Resolution Imaging
   Spectroradiometer fire counts in the southeastern U.S.
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GROUND-LEVEL PM2.5; AEROSOL OPTICAL-THICKNESS; UNITED-STATES;
   AIR-QUALITY; MODIS; US; RETRIEVALS; IMPACTS
AB Multiple studies have developed surface PM2.5 (particle size less than 2.5 mu m in aerodynamic diameter) prediction models using satellite-derived aerosol optical depth as the primary predictor and meteorological and land use variables as secondary variables. To our knowledge, satellite-retrieved fire information has not been used for PM2.5 concentration prediction in statistical models. Fire data could be a useful predictor since fires are significant contributors of PM2.5. In this paper, we examined whether remotely sensed fire count data could improve PM2.5 prediction accuracy in the southeastern U. S. in a spatial statistical model setting. A sensitivity analysis showed that when the radius of the buffer zone centered at each PM2.5 monitoring site reached 75 km, fire count data generally have the greatest predictive power of PM2.5 across the models considered. Cross validation (CV) generated an R-2 of 0.69, a mean prediction error of 2.75 mu g/m(3), and root-mean-square prediction errors (RMSPEs) of 4.29 mu g/m(3), indicating a good fit between the dependent and predictor variables. A comparison showed that the prediction accuracy was improved more substantially from the nonfire model to the fire model at sites with higher fire counts. With increasing fire counts, CV RMSPE decreased by values up to 1.5 mu g/m(3), exhibiting a maximum improvement of 13.4% in prediction accuracy. Fire count data were shown to have better performance in southern Georgia and in the spring season due to higher fire occurrence. Our findings indicate that fire count data provide a measurable improvement in PM2.5 concentration estimation, especially in areas and seasons prone to fire events.
C1 [Hu, Xuefei; Liu, Yang] Emory Univ, Dept Environm Hlth, Rollins Sch Publ Hlth, Atlanta, GA 30322 USA.
   [Waller, Lance A.] Emory Univ, Dept Biostat & Bioinformat, Rollins Sch Publ Hlth, Atlanta, GA 30322 USA.
   [Lyapustin, Alexei; Wang, Yujie] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Wang, Yujie] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Catonsville, MD USA.
RP Liu, Y (reprint author), Emory Univ, Dept Environm Hlth, Rollins Sch Publ Hlth, Atlanta, GA 30322 USA.
EM yang.liu@emory.edu
FU NASA Applied Sciences Program [NNX09AT52G, NNX11AI53G]; USEPA [R834799]
FX This work was partially supported by NASA Applied Sciences Program
   (grants NNX09AT52G and NNX11AI53G, PI: Liu). In addition, this
   publication was made possible by USEPA grant R834799. Its contents are
   solely the responsibility of the grantee and do not necessarily
   represent the official views of the USEPA. Further, USEPA does not
   endorse the purchase of any commercial products or services mentioned in
   the publication. PM2.5, meteorological, land use, and fire data used in
   this paper are available free through the links provided in section 2 of
   the paper. Inquiries regarding the MAIAC data should be directed to
   Alexei Lyapustin (alexei.i.lyapustin@nasa.gov) at the NASA Goddard Space
   Flight Center.
NR 30
TC 3
Z9 3
U1 2
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 OCT 16
PY 2014
VL 119
IS 19
BP 11375
EP 11386
DI 10.1002/2014JD021920
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS1PU
UT WOS:000344053400024
ER

PT J
AU Damiani, A
   Funke, B
   Puertas, ML
   Gardini, A
   von Clarmann, T
   Santee, ML
   Froidevaux, L
   Cordero, RR
AF Damiani, Alessandro
   Funke, Bernd
   Puertas, Manuel Lopez
   Gardini, Angela
   von Clarmann, Thomas
   Santee, Michelle L.
   Froidevaux, Lucien
   Cordero, Raul R.
TI Changes in the composition of the northern polar upper stratosphere in
   February 2009 after a sudden stratospheric warming
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SOLAR PROTON EVENTS; MIDDLE ATMOSPHERE; ODD NITROGEN; OZONE;
   TEMPERATURE; MIPAS; O-3; JANUARY; GOMOS/ENVISAT; VARIABILITY
AB Variability in the chemistry of the upper stratosphere/lowermesosphere region has been analyzed focusing on high latitudes during the boreal winter in 2009 characterized by the strong sudden stratospheric warming (SSW) on 24 January. Data from Michelson Interferometer for Passive Atmospheric Sounding aboard Envisat and the Microwave Limb Sounder on Aura have been used to exemplify these changes. Record high (low) values of O-3 and ClO (temperature and HCl) for the winters of 2005-2012, coupled with a simultaneous enhancement of ClONO2, have been observed in February 2009. This suggests that the very low temperatures favor a more effective ozone production and a greater O-3/O ratio. The latter is the main factor controlling active chlorine partitioning. Increases of ClO lead to high ClONO2 concentrations in the upper stratosphere at high latitudes, where its photodissociation rate is smaller. Since this increase of ClONO2 happens at the expense of HCl, the region of high ClONO2 roughly coincides with the region of low HCl. Although this period was characterized by an elevated stratopause event, the investigated region was not influenced by the descent of mesospheric air rich in NOx. Some limited enhancements in NOx at similar to 1 hPa occurred at latitudes greater than 80 degrees N after about 20 February, but they became consistent only in March. Intrusion of midlatitude air mostly occurred between the SSW and early February. Then, the sum of volume mixing ratios of ClONO2 + ClO + HCl remained approximately constant and close to the values of the other years. In contrast, it was up to 0.2 ppbv lower during the SSW period. These atypical chemical conditions occurred also in February 2006, but 2009 stands out for its long-lasting effects, which persisted until late March.
C1 [Damiani, Alessandro; Cordero, Raul R.] Univ Santiago Chile, Dept Phys, Santiago, Chile.
   [Funke, Bernd; Puertas, Manuel Lopez; Gardini, Angela] CSIC, Inst Astrofis Andalucia, Granada, Spain.
   [von Clarmann, Thomas] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76021 Karlsruhe, Germany.
   [Santee, Michelle L.; Froidevaux, Lucien] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Damiani, A (reprint author), Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa, Japan.
EM alecarlo.damiani@gmail.com
RI Funke, Bernd/C-2162-2008; Lopez Puertas, Manuel/M-8219-2013
OI Funke, Bernd/0000-0003-0462-4702; Lopez Puertas,
   Manuel/0000-0003-2941-7734
FU USACH-DICYT; FONDEF [IT13110034]; FONDECYT [1140239]; SOUSEI program,
   MEXT, JAPAN; NASA; Spanish MCINN [AYA2011-23552]; EC FEDER
FX The support of USACH-DICYT, FONDEF (IT13110034), and FONDECYT (1140239)
   is gratefully acknowledged. A.D. was also supported by the SOUSEI
   program, MEXT, JAPAN. Work at the Jet Propulsion Laboratory, California
   Institute of Technology, was done under contract with NASA. The IAA team
   was supported by the Spanish MCINN under grant AYA2011-23552 and EC
   FEDER funds. IMK/IAA-generated MIPAS/Envisat data can be obtained by
   registered users from the data server:
   http://www.imk-asf.kit.edu/english/308.php. MLS/Aura data are available
   at the Jet Propulsion Laboratory MLS website:
   http://mls.jpl.nasa.gov/index.php.
NR 55
TC 3
Z9 3
U1 2
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD OCT 16
PY 2014
VL 119
IS 19
BP 11429
EP 11444
DI 10.1002/2014JD021698
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS1PU
UT WOS:000344053400028
ER

PT J
AU Schroeder, JR
   Pan, LL
   Ryerson, T
   Diskin, G
   Hair, J
   Meinardi, S
   Simpson, I
   Barletta, B
   Blake, N
   Blake, DR
AF Schroeder, Jason R.
   Pan, Laura L.
   Ryerson, Tom
   Diskin, Glenn
   Hair, Johnathan
   Meinardi, Simone
   Simpson, Isobel
   Barletta, Barbara
   Blake, Nicola
   Blake, Donald R.
TI Evidence of mixing between polluted convective outflow and stratospheric
   air in the upper troposphere during DC3
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID VOLATILE ORGANIC-COMPOUNDS; DIODE-LASER HYGROMETER; UNITED-STATES;
   TROPOPAUSE FOLD; EXTRATROPICAL TROPOPAUSE; NONMETHANE HYDROCARBONS;
   POTENTIAL VORTICITY; DEEP CONVECTION; OZONE LAYERS; GEOS-CHEM
AB Aircraft measurements, including non-methane hydrocarbons (NMHCs), long-lived halocarbons, carbonmonoxide (CO), and ozone (O-3) collected on board the NASA DC-8 during the Deep Convection, Clouds, and Chemistry (DC3) field campaign (May - June 2012), were used to investigate interactions and mixing between stratospheric intrusions and polluted air masses. Stratospherically influenced air masses were detected using a suite of long-lived halocarbons, including chlorofluorocarbons (CFCs) and HCFCs, as a tracer for stratospheric air. A large number of stratospherically influenced samples were found to have reduced levels of O-3 and elevated levels of CO (both relative to background stratospheric air), indicative of mixing with anthropogenically influenced air. Using n-butane and propane as further tracers of anthropogenically influenced air, we show that this type of mixing was present both at low altitudes and in the upper troposphere (UT). At low altitudes, this mixing resulted in O-3 enhancements consistent with those reported at surface sites during deep stratospheric intrusions, while in the UT, two case studies were performed to identify the process by which this mixing occurs. In the first case study, stratospheric air was found to be mixed with aged outflow from a convective storm, while in the second case study, stratospheric air was found to have mixed with outflow from an active storm occurring in the vicinity of a stratospheric intrusion. From these analyses, we conclude that deep convective events may facilitate the mixing between stratospheric air and polluted boundary layer air in the UT. Throughout the entire DC3 study region, this mixing was found to be prevalent: 72% of all samples that involve stratosphere-troposphere mixing show influence of polluted air. Applying a simple chemical kinetics analysis to these data, we show that during DC3, the instantaneous production of hydroxyl radical (OH) in these mixed stratospheric-polluted air masses was 11 +/- 8 times higher than that of stratospheric air, and 4.2 +/- 1.8 times higher than that of background upper tropospheric air.
C1 [Schroeder, Jason R.; Meinardi, Simone; Simpson, Isobel; Barletta, Barbara; Blake, Nicola; Blake, Donald R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA.
   [Pan, Laura L.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
   [Ryerson, Tom] NOAA, Earth Syst Res Lab, Boulder, CO USA.
   [Diskin, Glenn; Hair, Johnathan] NASA, Langley Res Ctr, Hampton, VA USA.
RP Schroeder, JR (reprint author), Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA.
EM schroedj@uci.edu
RI Chem, GEOS/C-5595-2014; Pan, Laura/A-9296-2008; Ryerson,
   Tom/C-9611-2009; Manager, CSD Publications/B-2789-2015
OI Pan, Laura/0000-0001-7377-2114; 
FU NASA [NNX12AB76G]
FX Data used in this paper can be accessed via the NASA Airborne Science
   Data for Atmospheric Composition website
   (http://www-air.larc.nasa.gov/cgi-bin/ArcView/dc3). This work was
   supported by NASA grant NNX12AB76G. We would like to thank all members
   of the DC3 science and planning teams for their work and assistance in
   the field. We also thank our colleagues at UCI-Brent Love, Gloria Liu,
   Josette Marrero, Greg Hartt, Yu-Hsin Hung, Charlie Hirsch, and Aaron
   Gartner-for their assistance in the laboratory. We also thank Owen R.
   Cooper for providing useful comments and providing a creative spark
   during the early stages of this work, as well as our reviewers for
   providing many useful comments that helped make this a better paper.
NR 63
TC 8
Z9 8
U1 1
U2 26
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 OCT 16
PY 2014
VL 119
IS 19
BP 11477
EP 11491
DI 10.1002/2014JD022109
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS1PU
UT WOS:000344053400031
ER

PT J
AU Konopka, D
   Errico, M
   Bahrami, P
   Johnson, M
   Hays, CC
AF Konopka, Daniel
   Errico, Michael
   Bahrami, Poyan
   Johnson, Michael
   Hays, Charles C.
TI Tetramethylguanidine as an Aqueous Alkaline Electrolyte for
   Electrochemical Devices with Pt and Pd
SO JOURNAL OF PHYSICAL CHEMISTRY C
LA English
DT Article
ID OXYGEN REDUCTION REACTION; KOUTECKY-LEVICH PLOTS; FUEL-CELLS;
   GUANIDONIUM CATIONS; ADSORPTION; PT(111); OXIDATION; PLATINUM; SURFACES;
   KINETICS
AB 1,1,3,3-Tetramethylguanidine (TMG) is an organic superbase which has recently found use as a primary functional group in alkaline anion exchange membranes (AAEM). In this study we demonstrate the potential of aqueous TMG alkaline electrolyte as a substitute for NaOH(aq)/KOH(aq) with greater chemical similarity to AAEM functional groups. The water redox activities of Pt and Pd electrodes in 0.1 M TMG and 0.1 M KOH are compared, while hydrogen evolution/oxidation reactions (HER/HOR) and the oxygen reduction reaction (ORR) are studied in depth. Aqueous TMG supports comparable redox activity to KOH of equal concentration, but modifies surface processes through potential-dependent adsorptive behaviors. Rotating electrode, capacitance, and slow polarization measurements suggest that TMG and its decomposition species delay and participate in HER. HOR on Pt resembles that of a perfectly flat (111) surface in KOH, while hydrogen absorption on Pd is significantly hindered. ORR activity is dependent upon overpotential on both electrodes. But unlike most acid and alkaline electrolytes, TMG appears to alter the reaction pathway on Pt toward a 1.5e route. We propose that native or modified analogues of TMG might be optimized for compatibility with various catalysts so as to be utilized in alkaline electrochemical devices in place of NaOH and KOH.
C1 [Konopka, Daniel; Errico, Michael; Bahrami, Poyan; Johnson, Michael; Hays, Charles C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Konopka, D (reprint author), Alligant Sci LLC, 640 Plaza Dr,Suite 120, Highlands Ranch, CO 80129 USA.
EM konopka@alumni.caltech.edu
FU Department of Energy [DE-PS36-08G098101]
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. We would like to thank our collaborators in
   the group of Dr. Yu Seung Kim at Los Alamos National Laboratory and
   acknowledge the support of the Department of Energy (DE-PS36-08G098101).
NR 41
TC 0
Z9 0
U1 5
U2 39
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1932-7447
J9 J PHYS CHEM C
JI J. Phys. Chem. C
PD OCT 16
PY 2014
VL 118
IS 41
BP 23768
EP 23776
DI 10.1021/jp5068473
PG 9
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
   Multidisciplinary
SC Chemistry; Science & Technology - Other Topics; Materials Science
GA AR1GL
UT WOS:000343333600038
ER

PT J
AU Chomiuk, L
   Linford, JD
   Yang, J
   O'Brien, TJ
   Paragi, Z
   Mioduszewski, AJ
   Beswick, RJ
   Cheung, CC
   Mukai, K
   Nelson, T
   Ribeiro, VARM
   Rupen, MP
   Sokoloski, JL
   Weston, J
   Zheng, Y
   Bode, MF
   Eyres, S
   Roy, N
   Taylor, GB
AF Chomiuk, Laura
   Linford, Justin D.
   Yang, Jun
   O'Brien, T. J.
   Paragi, Zsolt
   Mioduszewski, Amy J.
   Beswick, R. J.
   Cheung, C. C.
   Mukai, Koji
   Nelson, Thomas
   Ribeiro, Valerio A. R. M.
   Rupen, Michael P.
   Sokoloski, J. L.
   Weston, Jennifer
   Zheng, Yong
   Bode, Michael F.
   Eyres, Stewart
   Roy, Nirupam
   Taylor, Gregory B.
TI Binary orbits as the driver of gamma-ray emission and mass ejection in
   classical novae
SO NATURE
LA English
DT Article
ID COMMON ENVELOPE PHASE; MERLIN OBSERVATIONS; MONOCEROTIS 2012; EVOLUTION;
   OUTBURST; RADIO; REMNANTS; MODELS; CYGNI; WINDS
AB Classical novae are the most common astrophysical thermonuclear explosions, occurring on the surfaces of white dwarf stars accreting gas from companions in binary star systems(1). Novae typically expel about 10(-4) solar masses of material at velocities exceeding 1,000 kilometres per second. However, the mechanism of mass ejection in novae is poorly understood, and could be dominated by the impulsive flash of thermonuclear energy(2), prolonged optically thick winds(3) or binary interaction with the nova envelope(4). Classical novae are now routinely detected at gigaelectronvolt gamma-ray wavelengths(5), suggesting that relativistic particles are accelerated by strong shocks in the ejecta. Here we report high-resolution radio imaging of the gamma-ray-emitting nova V959 Mon. We find that its ejecta were shaped by the motion of the binary system: some gas was expelled rapidly along the poles as a wind from the white dwarf, while denser material drifted out along the equatorial plane, propelled by orbital motion(6,7). At the interface between the equatorial and polar regions, we observe synchrotron emission indicative of shocks and relativistic particle acceleration, thereby pinpointing the location of gamma-ray production. Binary shaping of the nova ejecta and associated internal shocks are expected to be widespread among novae(8), explaining why many novae are gamma-ray emitters(5).
C1 [Chomiuk, Laura; Linford, Justin D.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
   [Yang, Jun] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
   [Yang, Jun; Paragi, Zsolt] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands.
   [Yang, Jun] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China.
   [O'Brien, T. J.; Beswick, R. J.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
   [Mioduszewski, Amy J.; Rupen, Michael P.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
   [Cheung, C. C.] Naval Res Lab, Space Sci Div, Washington, DC 20375 USA.
   [Mukai, Koji] Univ Maryland Baltimore Cty, Sch Phys & Astron, Baltimore, MD 21250 USA.
   [Mukai, Koji] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
   [Mukai, Koji] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
   [Nelson, Thomas] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
   [Ribeiro, Valerio A. R. M.] Univ Cape Town, Dept Astron, Astrophys Cosmol & Grav Ctr, ZA-7701 Rondebosch, South Africa.
   [Rupen, Michael P.] Natl Res Council Canada, Herzberg Astron & Astrophys, Penticton, BC V2A 6J9, Canada.
   [Sokoloski, J. L.; Weston, Jennifer; Zheng, Yong] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Bode, Michael F.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
   [Eyres, Stewart] Univ Cent Lancashire, Jeremiah Horrocks Inst Math Phys & Astron, Preston PR1 2HE, Lancs, England.
   [Roy, Nirupam] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
   [Taylor, Gregory B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
RP Chomiuk, L (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
EM chomiuk@pa.msu.edu
FU European Commission [283393, RI-261525]; Moore Foundation; Norris
   Foundation; McDonnell Foundation; Associates of the California Institute
   of Technology; University of Chicago; state of California; state of
   Illinois; state of Maryland; NSF; NASA [DPR S-15633-Y,
   10-FERMI10-C4-0060, NNX13AO91G]; NSF [AST-1211778]; South African SKA
   Project; Alexander von Humboldt Foundation
FX The National Radio Astronomy Observatory (NRAO) is a facility of the US
   National Science Foundation (NSF) operated under cooperative agreement
   by Associated Universities, Inc. The EVN is a joint facility of
   European, Chinese, South African and other radio astronomy institutes
   funded by their respective national research councils. The EVN and
   e-VLBI research infrastructures were supported by the European
   Commission Seventh Framework Programme (FP/2007-2013) under grant
   agreements nos 283393 (RadioNet3) and RI-261525 (NEXPReS). e-MERLIN is
   operated by The University of Manchester at Jodrell Bank Observatory on
   behalf of the Science and Technology Facilities Council. The SMA is a
   joint project between the Smithsonian Astrophysical Observatory and the
   Academia Sinica Institute of Astronomy and Astrophysics. Support for
   CARMA construction came from the Moore Foundation, the Norris
   Foundation, the McDonnell Foundation, the Associates of the California
   Institute of Technology, the University of Chicago, the states of
   California, Illinois and Maryland, and the NSF. Ongoing CARMA
   development and operations are supported by the NSF and by the CARMA
   partner universities. L.C. is a Jansky Fellow of the NRAO. This research
   received funding from NASA programmes DPR S-15633-Y and
   10-FERMI10-C4-0060 (C.C.C.), NASA award NNX13AO91G (T.N.), NSF award
   AST-1211778 (J.L.S. and J.W.), the South African SKA Project
   (V.A.R.M.R.) and the Alexander von Humboldt Foundation (N.R.).
NR 38
TC 19
Z9 19
U1 0
U2 13
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 OCT 16
PY 2014
VL 514
IS 7522
BP 339
EP +
DI 10.1038/nature13773
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AQ7JH
UT WOS:000342988600045
PM 25296250
ER

PT J
AU Lau, KY
   Lutes, GF
   Tjoelker, RL
AF Lau, Kam Y.
   Lutes, George F.
   Tjoelker, Robert L.
TI Ultra-Stable RF-Over-Fiber Transport in NASA Antennas, Phased Arrays and
   Radars
SO JOURNAL OF LIGHTWAVE TECHNOLOGY
LA English
DT Article
DE Arrays; deep space antennas; planetary radar imaging; space-borne radars
ID OPTICAL-FIBER; PERFORMANCE; FREQUENCY
AB Research and development in ultra-stable RF transport in optical fibers in the late-1970s/early-1980s at the NASA Jet Propulsion Laboratory led to successful field deployments in the three global sites of the NASA Deep Space Network which have been in continuous operation for the past three decades. This RF-over-fiber system underpinned critical tracking, navigation and communications functions for every deep space mission during this period and into the future. Successful operation of this system led to adoption of RF photonics as a fundamental infrastructure technology incorporated today in every deep space tracking antenna network and radio telescope worldwide. This RF-over-fiber system is also deployed in NASA's ground-based and space-borne planetary imaging and mapping radars. These systems were a predecessor to commercial RF-over-fiber networks which are key infrastructure components of today's cable and wireless industries. This paper provides an exposition of a number of NASA antennas, arrays and radar systems in which RF-over-fiber transport has played an enabling role.
C1 [Lau, Kam Y.] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 91125 USA.
   [Lutes, George F.; Tjoelker, Robert L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
FU Interplanetary Network Directorate
FX This work was performed by all authors at the Jet Propulsion Laboratory
   under the support of the Interplanetary Network Directorate.
NR 50
TC 11
Z9 12
U1 1
U2 8
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0733-8724
EI 1558-2213
J9 J LIGHTWAVE TECHNOL
JI J. Lightwave Technol.
PD OCT 15
PY 2014
VL 32
IS 20
SI SI
BP 3440
EP 3451
DI 10.1109/JLT.2014.2312930
PG 12
WC Engineering, Electrical & Electronic; Optics; Telecommunications
SC Engineering; Optics; Telecommunications
GA AX1JH
UT WOS:000346703000009
ER

PT J
AU Campbell, JF
   Lin, B
   Nehrir, AR
   Harrison, FW
   Obland, MD
AF Campbell, Joel F.
   Lin, Bing
   Nehrir, Amin R.
   Harrison, F. Wallace
   Obland, Michael D.
TI High-resolution CW lidar altimetry using repeating intensity-modulated
   waveforms and Fourier transform reordering
SO OPTICS LETTERS
LA English
DT Article
ID CO2 COLUMN MEASUREMENTS; LASER SYSTEM
AB An interpolation method is described for range measurements of high precision and altimetry using repeating intensity-modulated continuous wave (IM-CW) lidar waveforms, where the range is determined by means of a cross-correlation between the digital form of the transmitted signal and the digitized return signal collected by the lidar receiver. This method uses reordering of the array elements in the frequency domain to convert a repeating synthetic pulse signal to single highly interpolated pulse. The computation of this processing is marginally greater than the correlation itself, as it only involves reordering of the correlation in the frequency domain, which makes it possible to implement this in a real time application. It is shown through theoretical arguments and flight-testing that this is a viable method for high-speed interpolated range measurements. Standard deviation is 0.75 m over water with only 350 mw of transmitted power at 2600 m.
C1 [Campbell, Joel F.; Lin, Bing; Nehrir, Amin R.; Harrison, F. Wallace; Obland, Michael D.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Campbell, JF (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM joel.f.campbell@nasa.gov
NR 10
TC 4
Z9 4
U1 0
U2 1
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 OCT 15
PY 2014
VL 39
IS 20
BP 6078
EP 6081
DI 10.1364/OL.39.006078
PG 4
WC Optics
SC Optics
GA AR9RF
UT WOS:000343912000074
PM 25361160
ER

PT J
AU Panday, PK
   Williams, CA
   Frey, KE
   Brown, ME
AF Panday, Prajjwal K.
   Williams, Christopher A.
   Frey, Karen E.
   Brown, Molly E.
TI Application and evaluation of a snowmelt runoff model in the Tamor River
   basin, Eastern Himalaya using a Markov Chain Monte Carlo (MCMC) data
   assimilation approach
SO HYDROLOGICAL PROCESSES
LA English
DT Article
DE snowmelt; hydrology; SRM; APHRODITE; MODIS snow; Himalaya; MCMC; data
   assimilation
ID CLIMATE-CHANGE; UNCERTAINTY ESTIMATION; WATER-RESOURCES; INFORMATION;
   CALIBRATION; MOUNTAINS; SCENARIOS; IMPACTS; TOWERS
AB Previous studies have drawn attention to substantial hydrological changes taking place in mountainous watersheds where hydrology is dominated by cryospheric processes. Modelling is an important tool for understanding these changes but is particularly challenging in mountainous terrain owing to scarcity of ground observations and uncertainty of model parameters across space and time. This study utilizes a Markov Chain Monte Carlo data assimilation approach to examine and evaluate the performance of a conceptual, degree-day snowmelt runoff model applied in the Tamor River basin in the eastern Nepalese Himalaya. The snowmelt runoff model is calibrated using daily streamflow from 2002 to 2006 with fairly high accuracy (average Nash-Sutcliffe metric similar to 0.84, annual volume bias<3%). The Markov Chain Monte Carlo approach constrains the parameters to which the model is most sensitive (e.g. lapse rate and recession coefficient) and maximizes model fit and performance. Model simulated streamflow using an interpolated precipitation data set decreases the fractional contribution from rainfall compared with simulations using observed station precipitation. The average snowmelt contribution to total runoff in the Tamor River basin for the 2002-2006 period is estimated to be 29.7 +/- 2.9% (which includes 4.2 +/- 0.9% from snowfall that promptly melts), whereas 70.3 +/- 2.6% is attributed to contributions from rainfall. On average, the elevation zone in the 4000-5500m range contributes the most to basin runoff, averaging 56.9 +/- 3.6% of all snowmelt input and 28.9 +/- 1.1% of all rainfall input to runoff. Model simulated streamflow using an interpolated precipitation data set decreases the fractional contribution from rainfall versus snowmelt compared with simulations using observed station precipitation. Model experiments indicate that the hydrograph itself does not constrain estimates of snowmelt versus rainfall contributions to total outflow but that this derives from the degree-day melting model. Lastly, we demonstrate that the data assimilation approach is useful for quantifying and reducing uncertainty related to model parameters and thus provides uncertainty bounds on snowmelt and rainfall contributions in such mountainous watersheds. Copyright (c) 2013 John Wiley & Sons, Ltd.
C1 [Panday, Prajjwal K.] Woods Hole Res Ctr, Falmouth, MA 02540 USA.
   [Williams, Christopher A.; Frey, Karen E.] Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA.
   [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Panday, PK (reprint author), Woods Hole Res Ctr, 149 Woods Hole Rd, Falmouth, MA 02540 USA.
EM ppanday@whrc.org
RI Brown, Molly/E-2724-2010; 
OI Brown, Molly/0000-0001-7384-3314; Panday, Prajjwal/0000-0002-1287-2004
FU NASA Earth and Space Science Fellowship [NNX10AO65H]
FX This research was funded in part by a NASA Earth and Space Science
   Fellowship (Grant No. NNX10AO65H). We would like to thank the Department
   of Hydrology and Meteorology, Government of Nepal for providing
   hydrometeorological data used in this study. We thank Dr. Trent Biggs
   and one anonymous reviewer for their constructive comments.
NR 45
TC 13
Z9 13
U1 12
U2 41
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0885-6087
EI 1099-1085
J9 HYDROL PROCESS
JI Hydrol. Process.
PD OCT 15
PY 2014
VL 28
IS 21
BP 5337
EP 5353
DI 10.1002/hyp.10005
PG 17
WC Water Resources
SC Water Resources
GA AQ3EA
UT WOS:000342670900003
ER

PT J
AU Seager, R
   Neelin, D
   Simpson, I
   Liu, HB
   Henderson, N
   Shaw, T
   Kushnir, Y
   Ting, MF
   Cook, B
AF Seager, Richard
   Neelin, David
   Simpson, Isla
   Liu, Haibo
   Henderson, Naomi
   Shaw, Tiffany
   Kushnir, Yochanan
   Ting, Mingfang
   Cook, Benjamin
TI Dynamical and Thermodynamical Causes of Large-Scale Changes in the
   Hydrological Cycle over North America in Response to Global Warming
SO JOURNAL OF CLIMATE
LA English
DT Article
ID ATMOSPHERIC CIRCULATION RESPONSE; ERA-INTERIM REANALYSIS; TROPICAL
   PRECIPITATION; MODEL PROJECTIONS; 20-1ST CENTURY; UNITED-STATES;
   CLIMATE; DROUGHT; CMIP5; HYDROCLIMATE
AB The mechanisms of model-projected atmospheric moisture budget change across North America are examined in simulations conducted with 22 models from phase 5 of the Coupled Model Intercomparison Project. Modern-day model budgets are validated against the European Centre for Medium-Range Weather Forecasts Interim Re-Analysis. In the winter half year transient eddies converge moisture across the continent while the mean flow wets the west from central California northward and dries the southwest. In the summer half year there is widespread mean flow moisture divergence across the west and convergence over the Great Plains that is offset by transient eddy divergence. In the winter half year the models project drying for the southwest and wetting to the north. Changes in the mean flow moisture convergence are largely responsible across the west but intensified transient eddy moisture convergence wets the northeast. In the summer half year widespread declines in precipitation minus evaporation (P E) are supported by mean flow moisture divergence across the west and transient eddy divergence in the Great Plains. The changes in mean flow convergence are related to increases in specific humidity but also depend on changes in the mean flow including increased low-level divergence in the U.S. Southwest and a zonally varying wave that wets the North American west and east coasts in winter and dries the U.S. Southwest. Increased transient eddy fluxes occur even as low-level eddy activity weakens and arise from strengthened humidity gradients. A full explanation of North American hydroclimate changes will require explanation of mean and transient circulation changes and the coupling between the moisture and circulation fields.
C1 [Seager, Richard; Simpson, Isla; Liu, Haibo; Henderson, Naomi; Shaw, Tiffany; Kushnir, Yochanan; Ting, Mingfang] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
   [Neelin, David] Univ Calif Los Angeles, Dept Atmospher Sci, Los Angeles, CA 90024 USA.
   [Cook, Benjamin] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Seager, R (reprint author), Columbia Univ, Lamont Doherty Earth Observ, 61 Route 9W, Palisades, NY 10964 USA.
EM seager@ldeo.columbia.edu
RI Cook, Benjamin/H-2265-2012
FU NOAA [NA10OAR4310137]; DOE [DE-SC0005107]; NSF [AGS-1243204, AGS-317469,
   AGS-1102838]
FX This work was supported by NOAA Award NA10OAR4310137 (Global Decadal
   Hydroclimate Variability and Change), DOE Award DE-SC0005107, and NSF
   Awards AGS-1243204, AGS-317469, and AGS-1102838 (JDN). We thank Dong Eun
   Lee for downloading the ERA-I data and ECMWF for making the reanalysis
   data available. 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 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. The moisture budget breakdowns analyzed
   here can be accessed at
   http://kage.ldeo.columbia.edu:81/expert/SOURCES/.LDEO/.ClimateGroup/.PRO
   JECTS/.IPCC/.CMIP5/.MoistureBudget/.
NR 40
TC 18
Z9 18
U1 4
U2 39
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 OCT 15
PY 2014
VL 27
IS 20
BP 7921
EP 7948
DI 10.1175/JCLI-D-14-00153.1
PG 28
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AQ5YB
UT WOS:000342883400024
ER

PT J
AU Rocha, C
   Munoz, C
AF Rocha, Camilo
   Munoz, Cesar
TI Synchronous set relations in rewriting logic
SO SCIENCE OF COMPUTER PROGRAMMING
LA English
DT Article; Proceedings Paper
CT 14th Brazilian Symposium on Formal Methods (SBMF)
CY SEP 26-30, 2011
CL Sao Paulo, BRAZIL
SP CNPq, Brazilian Sci & Technol Res Council, CAPES, Brazilian Higher Educ Fund Council, FAPESP, Sao Paulo Res Fdn, Google Inc, Univ Sao Paulo, Univ Presbiteriana Mackenzie
DE Synchronous set relations; Synchronous semantics; Rewriting logic;
   Formal simulation and verification; PLEXIL
ID P SYSTEMS
AB This paper presents a mathematical foundation and a rewriting logic infrastructure for the execution and property verification of synchronous set relations. The mathematical foundation is given in the language of abstract set relations. The infrastructure, which is written in the Maude system, enables the synchronous execution of a set relation provided by the user. By using the infrastructure, algorithm verification techniques such as reachability analysis and model checking, already available in Maude for traditional asynchronous rewriting, are automatically available to synchronous set rewriting. In this way, set-based synchronous languages and systems such as those built from agents, components, or objects can be naturally specified and simulated, and are also amenable to formal verification in the Maude system. The use of the infrastructure and some of its Maude-based verification capabilities are illustrated with an executable operational semantics of the Plan Execution Interchange Language (PLEXIL), a synchronous language developed by NASA to support autonomous spacecraft operations. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Rocha, Camilo] Escuela Colombiana Ingn, Bogota, DC, Colombia.
   [Munoz, Cesar] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Rocha, C (reprint author), Escuela Colombiana Ingn, Bogota, DC, Colombia.
EM camilo.rocha@escuelaing.edu.co; cesar.a.munoz@nasa.gov
NR 20
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-6423
EI 1872-7964
J9 SCI COMPUT PROGRAM
JI Sci. Comput. Program.
PD OCT 15
PY 2014
VL 92
BP 211
EP 228
DI 10.1016/j.scico.2013.07.008
PN B
PG 18
WC Computer Science, Software Engineering
SC Computer Science
GA AK7HA
UT WOS:000338598100007
ER

PT J
AU Noriega-Crespo, A
   Raga, AC
   Moro-Martin, A
   Flagey, N
   Carey, SJ
AF Noriega-Crespo, A.
   Raga, A. C.
   Moro-Martin, A.
   Flagey, N.
   Carey, S. J.
TI Proper motions of young stellar outflows in the mid-infrared with
   Spitzer II HH 377/Cep E
SO NEW JOURNAL OF PHYSICS
LA English
DT Article
DE ISM: jets and outflows; infrared: ISM; Herbig-Haro objects;
   circumstellar matter; star formation
ID HERBIG-HARO FLOWS; CEPHEUS-E OUTFLOW; SHOCK-WAVES; PROTOSTELLAR JETS;
   MOLECULAR CLOUDS; NGC 1333; CEP E; H-2; SYSTEM; EVOLUTION
AB We have used multiple mid-infrared observations at 4.5 mu m obtained with the infrared array camera, of the compact(similar to 1.4') young stellar bipolar outflow Cep E to measure the proper motion of its brightest condensations. The images span a period of similar to 6 yr and have been reprocessed to achieve a higher angular resolution (similar to 0.8 '') than their normal beam(similar to 2 ''). We found that for a distance of 730 pc, the tangential velocities of the north and south outflow lobes are 62 +/- 29 and 94 +/- 26 km s(-1) respectively, and moving away from the central source roughly along the major axis of the flow. A simple 3D hydrodynamical simulation of the H-2 gas in a precessing outflow supports this idea. Observations and models confirm that the molecular hydrogen gas, traced by the pure rotational transitions, moves at highly supersonic velocities without being dissociated. This suggests either a very efficient mechanism to reform H-2 molecules along these shocks or the presence of some other mechanism (e. g. strong magnetic field) that shields the H-2 gas.
C1 [Noriega-Crespo, A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
   [Raga, A. C.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico.
   [Noriega-Crespo, A.; Moro-Martin, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Flagey, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91099 USA.
   [Carey, S. J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
   [Flagey, N.] Inst Astron, Hilo, HI 96720 USA.
RP Noriega-Crespo, A (reprint author), CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
EM anoriega@stsci.edu
FU Spitzer Space Telescope (NASA) [1407]; National Aeronautics and Space
   Administration (NASA)
FX The authors thank the referees and editors for their careful reading of
   the manuscript and their valuable suggestions; in particular the
   realization that rotational H<INF>2</INF> can trace higher kinetic
   temperatures than the vibrational ones. This research is based in part
   on observations made with the Spitzer Space Telescope (NASA contract
   1407) and has made use of the NASA/IPAC Infrared Science Archive, both
   are operated by the Jet Propulsion Laboratory, California Institute of
   Technology, under contract with the National Aeronautics and Space
   Administration (NASA).
NR 67
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 OCT 14
PY 2014
VL 16
AR 105008
DI 10.1088/1367-2630/16/10/105008
PG 15
WC Physics, Multidisciplinary
SC Physics
GA AS2GS
UT WOS:000344098400002
ER

PT J
AU Zevalkink, A
   Zeier, WG
   Cheng, E
   Snyder, J
   Fleurial, JP
   Bux, S
AF Zevalkink, Alex
   Zeier, Wolfgang G.
   Cheng, Ethan
   Snyder, Jeffrey
   Fleurial, Jean-Pierre
   Bux, Sabah
TI Nonstoichiometry in the Zintl Phase Yb1-delta Zn2Sb2 as a Route to
   Thermoelectric Optimization
SO CHEMISTRY OF MATERIALS
LA English
DT Article
ID THERMAL-CONDUCTIVITY; SOLID-SOLUTIONS; CAAL2SI2; CRYSTAL; CHAINS;
   TRANSITION; EFFICIENCY; CHEMISTRY; CACD2SB2; METAL
AB Classically, Zintl phases are defined as valence-precise line compounds and are thus expected to exhibit intrinsic semiconducting behavior. Contradicting this definition are AZn(2)Sb(2) Zintl compounds (A = Ca, Sr, Eu, Yb), which exhibit metallic behavior due to high concentrations of cation vacancies, according to recent density functional calculations. Here, we use synchrotron diffraction and high-temperature electronic and thermal transport properties to show that the phase width of Yb1-delta Zn2Sb2 is wide enough to allow for significant variation and optimization of the thermoelectric properties within the single phase region. Samples with nominal compositions of YbxZn2Sb2 (0.98 < x < 1.05) were synthesized using a solid-state process. With decreasing synthetic Yb content, synchrotron X-ray diffiaction reveals decreased lattice parameters, decreased occupancy of the Yb site, and a relaxation of the tetrahedral angles within the Zn2Sb2 sheets. In Yb-deficient samples, the carrier concentration can be controlled by varying x, whereas, in samples with excess Yb, the carrier concentration remains constant and p-type. Fully intrinsic semiconducting behavior was not obtained, suggesting that a slightly Yb-deficient composition is thermodynamically preferable to the valence-precise stoichiometry of delta = 0. Tuning the vacancy concentration provides a new route to controlling the electronic properties in Yb1-delta Zn2Sb2 and leads to a SO% improvement in the thermoelectric figure of merit (zT = 0.85 at 773 K) compared to previously reported values for unalloyed YbZn2Sb2.
C1 [Zevalkink, Alex; Zeier, Wolfgang G.; Snyder, Jeffrey] CALTECH, Pasadena, CA 91125 USA.
   [Zevalkink, Alex; Cheng, Ethan; Fleurial, Jean-Pierre; Bux, Sabah] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Snyder, J (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM jsnyder@caltech.edu; sabah.k.bux@jpl.nasa.gov
RI Snyder, G. Jeffrey/E-4453-2011; Zeier, Wolfgang/N-2562-2014
OI Snyder, G. Jeffrey/0000-0003-1414-8682; 
FU National Aeronautics and Space Administration; NASA Science Missions
   Directorate's Radioisotope Power Systems Technology Advancement Program;
   U.S. Department of Energy, Office of Science, Office of Basic Energy
   Sciences [DE-AC02-06CH11357]
FX This work was performed at the Jet Propulsion Laboratory, California
   Institute of Technology under contract with the National Aeronautics and
   Space Administration. This work was supported by the NASA Science
   Missions Directorate's Radioisotope Power Systems Technology Advancement
   Program. We gratefully acknowledge Gregory Gerig for performing Seebeck
   measurements. 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.
NR 49
TC 18
Z9 18
U1 2
U2 39
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 OCT 14
PY 2014
VL 26
IS 19
BP 5710
EP 5717
DI 10.1021/cm502588r
PG 8
WC Chemistry, Physical; Materials Science, Multidisciplinary
SC Chemistry; Materials Science
GA AQ9SI
UT WOS:000343195600039
ER

PT J
AU Stephenson, JH
   Tinney, CE
   Greenwood, E
   Watts, ME
AF Stephenson, James H.
   Tinney, Charles E.
   Greenwood, Eric
   Watts, Michael E.
TI Time frequency analysis of sound from a maneuvering rotorcraft
SO JOURNAL OF SOUND AND VIBRATION
LA English
DT Article
ID VORTEX INTERACTION NOISE; WAVELET ANALYSIS; TURBULENCE
AB The acoustic signatures produced by a full-scale, Bell 430 helicopter during steady-level-flight and transient roll-right maneuvers are analyzed by way of time-frequency analysis. The roll-right maneuvers comprise both a medium and a fast roll rate. Data are acquired using a single ground based microphone that are analyzed by way of the Morlet wavelet transform to extract the spectral properties and sound pressure levels as functions of time. The findings show that during maneuvering operations of the helicopter, both the overall sound pressure level and the blade-vortex interaction sound pressure level are greatest when the roll rate of the vehicle is at its maximum. The reduced inflow in the region of the rotor disk where blade-vortex interaction noise originates is determined to be the cause of the increase in noise. A local decrease in inflow reduces the miss distance of the tip vortex and thereby increases the BVI noise signature. Blade loading and advance ratios are also investigated as possible mechanisms for increased sound production, but are shown to be fairly constant throughout the maneuvers. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Stephenson, James H.; Tinney, Charles E.] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Ctr Aeromech Res, Austin, TX 78712 USA.
   [Greenwood, Eric; Watts, Michael E.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Stephenson, JH (reprint author), Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Ctr Aeromech Res, Austin, TX 78712 USA.
EM j.stephenson@utexas.edu; cetinney@utexas.edu
RI Greenwood, Eric/Q-7642-2016
OI Greenwood, Eric/0000-0002-0427-539X
FU DoD
FX The flight test data was acquired during a joint test program between
   NASA Langley Research Center, Bell Helicopter Textron and the US Army
   Aeroflightdynamics Directorate. JHS would also like to thank the DoD for
   funding provided through the SMART Fellowship program.
NR 24
TC 3
Z9 3
U1 3
U2 8
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 OCT 13
PY 2014
VL 333
IS 21
BP 5324
EP 5339
DI 10.1016/j.jsv.2014.05.018
PG 16
WC Acoustics; Engineering, Mechanical; Mechanics
SC Acoustics; Engineering; Mechanics
GA AN0VC
UT WOS:000340301100007
ER

PT J
AU Evans, PA
   Willingale, R
   Osborne, JP
   O'Brien, PT
   Tanvir, NR
   Frederiks, DD
   Pal'shin, VD
   Svinkin, DS
   Lien, A
   Cummings, J
   Xiong, S
   Zhang, BB
   Gotz, D
   Savchenko, V
   Negoro, H
   Nakahira, S
   Suzuki, K
   Wiersema, K
   Starling, RLC
   Castro-Tirado, AJ
   Beardmore, AP
   Sanchez-Ramirez, R
   Gorosabel, J
   Jeong, S
   Kennea, JA
   Burrows, DN
   Gehrels, N
AF Evans, P. A.
   Willingale, R.
   Osborne, J. P.
   O'Brien, P. T.
   Tanvir, N. R.
   Frederiks, D. D.
   Pal'shin, V. D.
   Svinkin, D. S.
   Lien, A.
   Cummings, J.
   Xiong, S.
   Zhang, B. -B.
   Goetz, D.
   Savchenko, V.
   Negoro, H.
   Nakahira, S.
   Suzuki, K.
   Wiersema, K.
   Starling, R. L. C.
   Castro-Tirado, A. J.
   Beardmore, A. P.
   Sanchez-Ramirez, R.
   Gorosabel, J.
   Jeong, S.
   Kennea, J. A.
   Burrows, D. N.
   Gehrels, N.
TI GRB 130925A: an ultralong gamma ray burst with a dust-echo afterglow,
   and implications for the origin of the ultralong GRBs
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gamma-ray burst: general; gamma-ray burst, individual: GRB 130925A
ID MASSIVE BLACK-HOLE; SWIFT XRT DATA; TIDAL DISRUPTION; STAR-FORMATION;
   LIGHT CURVES; PHYSICAL ORIGINS; GALACTIC NUCLEI; COMPLETE SAMPLE; HOST
   GALAXIES; LONG
AB GRB 130925A was an unusual gamma ray burst (GRB), consisting of three distinct episodes of high-energy emission spanning similar to 20 ks, making it a member of the proposed category of 'ultralong' bursts. It was also unusual in that its late-time X-ray emission observed by Swift was very soft, and showed a strong hard-to-soft spectral evolution with time. This evolution, rarely seen in GRB afterglows, can be well modelled as the dust-scattered echo of the prompt emission, with stringent limits on the contribution from the normal afterglow (i.e. external shock) emission. We consider and reject the possibility that GRB 130925A was some form of tidal disruption event, and instead show that if the circumburst density around GRB 130925A is low, the long duration of the burst and faint external shock emission are naturally explained. Indeed, we suggest that the ultralong GRBs as a class can be explained as those with low circumburst densities, such that the deceleration time (at which point the material ejected from the nascent black hole is decelerated by the circumburst medium) is similar to 20 ks, as opposed to a few hundred seconds for the normal long GRBs. The increased deceleration radius means that more of the ejected shells can interact before reaching the external shock, naturally explaining both the increased duration of GRB 130925A, the duration of its prompt pulses, and the fainter-than-normal afterglow.
C1 [Evans, P. A.; Willingale, R.; Osborne, J. P.; O'Brien, P. T.; Tanvir, N. R.; Wiersema, K.; Starling, R. L. C.; Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
   [Frederiks, D. D.; Pal'shin, V. D.; Svinkin, D. S.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia.
   [Lien, A.; Cummings, J.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Lien, A.; Cummings, J.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
   [Lien, A.; Cummings, J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
   [Lien, A.; Cummings, J.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
   [Xiong, S.; Zhang, B. -B.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
   [Goetz, D.] Univ Paris Diderot, CE Saclay, CEA DSM Irfu CNRS, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France.
   [Savchenko, V.] Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, Francois Arago Ctr,APC,CNRS IN2P3,CEA Irfu, F-75205 Paris 13, France.
   [Negoro, H.; Suzuki, K.] Nihon Univ, Dept Phys, Chiyoda Ku, Tokyo 1018308, Japan.
   [Nakahira, S.] Aerosp Explorat Agcy JAXA, ISAS, ISS Sci Project Off, Tsukuba, Ibaraki 3058505, Japan.
   [Castro-Tirado, A. J.; Sanchez-Ramirez, R.; Gorosabel, J.; Jeong, S.] CSIC, IAA, E-18008 Granada, Spain.
   [Castro-Tirado, A. J.] Univ Malaga, ETS Ingenieros Ind, Unidad Asociada Dept Ingn Sistemas & Automat, E-29071 Malaga, Spain.
   [Gorosabel, J.] Univ Pais Vasco UPV EHU, ETS, Unidad Asociada Grp Ciencias Planetarias UPV EHU, Dept Fis Aplicada 1, E-48013 Bilbao, Spain.
   [Gorosabel, J.] Ikerbasque, Basque Fdn Sci, E-48008 Bilbao, Spain.
   [Kennea, J. A.; Burrows, D. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Evans, PA (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
EM pae9@leicester.ac.uk
RI Pal'shin, Valentin/F-3973-2014; Svinkin, Dmitry/C-1934-2014; Zhang,
   Binbin/C-9035-2013; 
OI Zhang, Binbin/0000-0003-2002-116X; Frederiks,
   Dmitry/0000-0002-1153-6340; Castro-Tirado, A. J./0000-0003-2999-3563
FU UK Space Agency; Russian Space Agency contract, RFBR [12-02-00032a,
   13-02-12017 ofi-m]; NASA [NAS5-00136]; Spanish Ministry project
   [AYA2012-29727-C03-01]
FX This work made use of data supplied by the UK Swift Science Data Centre
   at the University of Leicester. PAE, JPO, KW and APB acknowledge UK
   Space Agency support. The Konus-Wind experiment is partially supported
   by a Russian Space Agency contract, RFBR grants 12-02-00032a and
   13-02-12017 ofi-m. DNB and JAK acknowledge support from NASA contract
   NAS5-00136. This work includes 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, in
   the island of La Palma. This work was partially supported by the Spanish
   Ministry project AYA2012-29727-C03-01.
NR 89
TC 23
Z9 23
U1 1
U2 11
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 OCT 11
PY 2014
VL 444
IS 1
BP 250
EP 267
DI 10.1093/mnras/stu1459
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ6LX
UT WOS:000342925100020
ER

PT J
AU Siwak, M
   Rucinski, SM
   Matthews, JM
   Guenther, DB
   Kuschnig, R
   Moffat, AFJ
   Rowe, JF
   Sasselov, D
   Weiss, WW
AF Siwak, Michal
   Rucinski, Slavek M.
   Matthews, Jaymie M.
   Guenther, David B.
   Kuschnig, Rainer
   Moffat, Anthony F. J.
   Rowe, Jason F.
   Sasselov, Dimitar
   Weiss, Werner W.
TI A stable quasi-periodic 4.18-d oscillation and mysterious occultations
   in the 2011 MOST light-curve of TW Hya
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion: accretion discs; stars: individual: TW Hya; stars: variables:
   T Tauri, Herbig Ae/Be
ID MAGNETIC NEUTRON-STARS; MAGNETOSPHERIC ACCRETION MODELS; DISK ACCRETION;
   TAURI STARS; MAGNETOHYDRODYNAMIC SIMULATIONS; AB-AURIGAE; X-RAY;
   VARIABILITY; HYDRAE; PHOTOMETRY
AB We present an analysis of the 2011 photometric observations of TW Hya by the MOST satellite; this is the fourth continuous series of this type. The large-scale light variations are dominated by a strong, quasi-periodic 4.18-d oscillation with superimposed, apparently chaotic flaring activity. The former is probably produced by stellar rotation with one large hotspot created by a stable accretion funnel, while the latter may be produced by small hotspots, created at moderate latitudes by unstable accretion tongues. A new, previously unnoticed feature is a series of semiperiodic, well-defined brightness dips of unknown nature, of which 19 were observed during 43 d of our nearly continuous observations. Re-analysis of the 2009 MOST light-curve revealed the presence of three similar dips. On the basis of recent theoretical results, we tentatively conclude that the dips may represent occultations of the small hotspots created by unstable accretion tongues by hypothetical optically thick clumps of dust.
C1 [Siwak, Michal] Cracov Pedag Univ, Mt Suhora Astron Observ, PL-30084 Cracov, Poland.
   [Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
   [Matthews, Jaymie M.; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
   [Guenther, David B.] St Marys Univ, Inst Computat Astrophys, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
   [Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
   [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
   [Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Siwak, M (reprint author), Cracov Pedag Univ, Mt Suhora Astron Observ, Ul Podchorazych 2, PL-30084 Cracov, Poland.
EM siwak@nac.oa.uj.edu.pl
FU Polish National Science Centre [2012/05/E/ST9/03915]; Natural Sciences
   and Engineering Research Council of Canada; FQRNT (Quebec); Canadian
   Space Agency; Austrian Science Funds [P22691-N16]
FX This study was based on data from the MOST satellite, a Canadian Space
   Agency mission jointly operated by Dynacon Inc., the University of
   Toronto Institute of Aerospace Studies, and the University of British
   Columbia, with the assistance of the University of Vienna. It also made
   use of NASA's Astrophysics Data System (ADS) Bibliographic Services. MS
   is grateful to the Polish National Science Centre for grant
   2012/05/E/ST9/03915, which fully supported his research. The Natural
   Sciences and Engineering Research Council of Canada supports the
   research of DBG, JMM, AFJM and SMR. Additional support for AFJM was
   provided by FQRNT (Quebec). RK is supported by the Canadian Space
   Agency, and WWW is supported by the Austrian Science Funds (P22691-N16).
   Special thanks also go to the anonymous referee for highly useful
   suggestions and comments on a previous version of this paper.
NR 36
TC 2
Z9 2
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 OCT 11
PY 2014
VL 444
IS 1
BP 327
EP 335
DI 10.1093/mnras/stu1304
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ6LX
UT WOS:000342925100025
ER

PT J
AU David-Uraz, A
   Wade, GA
   Petit, V
   ud-Doula, A
   Sundqvist, JO
   Grunhut, J
   Shultz, M
   Neiner, C
   Alecian, E
   Henrichs, HF
   Bouret, JC
AF David-Uraz, A.
   Wade, G. A.
   Petit, V.
   ud-Doula, A.
   Sundqvist, J. O.
   Grunhut, J.
   Shultz, M.
   Neiner, C.
   Alecian, E.
   Henrichs, H. F.
   Bouret, J. -C.
CA MiMeS Collaboration
TI Investigating the origin of cyclical wind variability in hot, massive
   stars - I. On the dipolar magnetic field hypothesis
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: magnetic field; stars: massive; stars: winds, outflows
ID O-TYPE STARS; COROTATING INTERACTION REGIONS; NARROW ABSORPTION
   COMPONENTS; DRIVEN STELLAR WINDS; IUE MEGA CAMPAIGN; TIME-SERIES;
   B-SUPERGIANTS; SPECTROPOLARIMETRIC OBSERVATIONS; DYNAMICAL SIMULATIONS;
   ZETA-OPHIUCHI
AB OB stars exhibit various types of spectral variability associated with wind structures, including the apparently ubiquitous discrete absorption components (DACs). These are proposed to be caused by either magnetic fields or non-radial pulsations. In this paper, we evaluate the possible relation between large-scale, dipolar magnetic fields and the DAC phenomenon by investigating the magnetic properties of a sample of 13 OB stars exhibiting well-documented DACbehaviour. Using high-precision spectropolarimetric data acquired in part in the context of theMagnetism in Massive Stars project, we find no evidence for surface dipolar magnetic fields in any of these stars. Using Bayesian inference, we compute upper limits on the strengths of the fields and use these limits to assess two potential mechanisms by which the field may influence wind outflow: magnetic wind confinement and local photospheric brightness enhancements. Within the limits we derive, both mechanisms fail to provide a systematic process capable of producing DACs in all of the stars of our sample. Therefore, this implies that dipolar fields are highly unlikely to be responsible for these structures in all massive stars, meaning that some other mechanism must come into play.
C1 [David-Uraz, A.; Wade, G. A.; Shultz, M.] Royal Mil Coll Canada, Dept Phys, Stn Forces, Kingston, ON K7K 4B4, Canada.
   [David-Uraz, A.; Shultz, M.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada.
   [Petit, V.; Sundqvist, J. O.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
   [ud-Doula, A.] Penn State Worthington Scranton, Dunmore, PA 18512 USA.
   [Sundqvist, J. O.] Univ Munich, Inst Astron & Astrophys, D-81679 Munich, Germany.
   [Grunhut, J.] European Org Astron Res Southern Hemisphere, D-85748 Garching, Germany.
   [Shultz, M.] European Org Astron Res Southern Hemisphere, Santiago 19, Chile.
   [Neiner, C.; Alecian, E.] Univ Paris Diderot, UPMC, Observ Paris, LESIA,UMR CNRS 8109, F-92195 Meudon, France.
   [Neiner, C.; Alecian, E.] Univ Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France.
   [Henrichs, H. F.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
   [Bouret, J. -C.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France.
   [Bouret, J. -C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP David-Uraz, A (reprint author), Royal Mil Coll Canada, Dept Phys, Stn Forces, POB 17000, Kingston, ON K7K 4B4, Canada.
EM adavid-uraz@astro.queensu.ca
OI Neiner, Coralie/0000-0003-1978-9809
FU Fonds quebecois de la recherche sur la nature et les technologies; NSERC
   Discovery Grant; NASA Chandra theory grant; NASA ATP Grant [NNX11AC40G]
FX ADU gratefully acknowledges the support of the Fonds quebecois de la
   recherche sur la nature et les technologies. GAW is supported by an
   NSERC Discovery Grant. AuD acknowledges support from the NASA Chandra
   theory grant to Penn State Worthington Scranton and NASA ATP Grant
   NNX11AC40G.
NR 66
TC 10
Z9 10
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 OCT 11
PY 2014
VL 444
IS 1
BP 429
EP 442
DI 10.1093/mnras/stu1458
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ6LX
UT WOS:000342925100034
ER

PT J
AU Acuner, Z
   Inam, SC
   Sahiner, S
   Serim, MM
   Baykal, A
   Swank, J
AF Acuner, Z.
   Inam, S. C.
   Sahiner, S.
   Serim, M. M.
   Baykal, A.
   Swank, J.
TI Timing studies of X Persei and the discovery of its transient
   quasi-periodic oscillation feature
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: neutron; pulsars: individual: X
   Persei; X-rays: binaries
ID PROPORTIONAL COUNTER ARRAY; RED POWER SPECTRA; RAY PULSARS; SAX
   J2103.5+4545; ACCRETION; RXTE; CALIBRATION; EMISSION; ORBIT; X-1
AB We present a timing analysis of X Persei (X Per) using observations made between 1998 and 2010 with the Proportional Counter Array (PCA) onboard the Rossi X-ray Timing Explorer (RXTE) and with the INTEGRAL Soft Gamma-Ray Imager (ISGRI). All pulse arrival times obtained from the RXTE-PCA observations are phase-connected and a timing solution is obtained using these arrival times. We update the long-term pulse frequency history of the source by measuring its pulse frequencies using RXTE-PCA and ISGRI data. From the RXTE-PCA data, the relation between the frequency derivative and X-ray flux suggests accretion via the companion's stellar wind. However, the detection of a transient quasi-periodic oscillation feature, peaking at similar to 0.2 Hz, suggests the existence of an accretion disc. We find that double-break models fit the average power spectra well, which suggests that the source has at least two different accretion flow components dominating the overall flow. From the power spectrum of frequency derivatives, we measure a power-law index of similar to-1, which implies that, on short time-scales, disc accretion dominates over noise, while on time-scales longer than the viscous time-scales, the noise dominates. From pulse profiles, we find a correlation between the pulse fraction and the count rate of the source.
C1 [Acuner, Z.; Sahiner, S.; Serim, M. M.; Baykal, A.] Middle E Tech Univ, Dept Phys, TR-06531 Ankara, Turkey.
   [Inam, S. C.] Baskent Univ, Dept Elect & Elect Engn, TR-06810 Ankara, Turkey.
   [Swank, J.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Acuner, Z (reprint author), Middle E Tech Univ, Dept Phys, TR-06531 Ankara, Turkey.
EM zeynepa@astroa.physics.metu.edu.tr
FU TUBITAK, the Scientific and Technological Research Council of Turkey
   [TBAG 109T748]
FX We acknowledge support from TUBITAK, the Scientific and Technological
   Research Council of Turkey through the research project TBAG 109T748. We
   thank Tod Strohmayer and Craig Markwardt for useful suggestions.
NR 35
TC 0
Z9 0
U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 11
PY 2014
VL 444
IS 1
BP 457
EP 465
DI 10.1093/mnras/stu1351
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ6LX
UT WOS:000342925100036
ER

PT J
AU Southworth, J
   Hinse, TC
   Burgdorf, M
   Novati, SC
   Dominik, M
   Galianni, P
   Gerner, T
   Giannini, E
   Gu, SH
   Hundertmark, M
   Jorgensen, UG
   Juncher, D
   Kerins, E
   Mancini, L
   Rabus, M
   Ricci, D
   Schaefer, S
   Skottfelt, J
   Tregloan-Reed, J
   Wang, XB
   Wertz, O
   Alsubai, KA
   Andersen, JM
   Bozza, V
   Bramich, DM
   Browne, P
   Ciceri, S
   D'Ago, G
   Damerdji, Y
   Diehl, C
   Dodds, P
   Elyiv, A
   Fang, XS
   Finet, F
   Jaimes, RF
   Hardis, S
   Harpsoe, K
   Jessen-Hansen, J
   Kains, N
   Kjeldsen, H
   Korhonen, H
   Liebig, C
   Lund, MN
   Lundkvist, M
   Mathiasen, M
   Penny, MT
   Popovas, A
   Prof, S
   Rahvar, S
   Sahu, K
   Scarpetta, G
   Schmidt, RW
   Schoenebeck, F
   Snodgrass, C
   Street, RA
   Surdej, J
   Tsapras, Y
   Vilela, C
AF Southworth, John
   Hinse, T. C.
   Burgdorf, M.
   Novati, S. Calchi
   Dominik, M.
   Galianni, P.
   Gerner, T.
   Giannini, E.
   Gu, S. -H.
   Hundertmark, M.
   Jorgensen, U. G.
   Juncher, D.
   Kerins, E.
   Mancini, L.
   Rabus, M.
   Ricci, D.
   Schaefer, S.
   Skottfelt, J.
   Tregloan-Reed, J.
   Wang, X. -B.
   Wertz, O.
   Alsubai, K. A.
   Andersen, J. M.
   Bozza, V.
   Bramich, D. M.
   Browne, P.
   Ciceri, S.
   D'Ago, G.
   Damerdji, Y.
   Diehl, C.
   Dodds, P.
   Elyiv, A.
   Fang, X. -S.
   Finet, F.
   Jaimes, R. Figuera
   Hardis, S.
   Harpsoe, K.
   Jessen-Hansen, J.
   Kains, N.
   Kjeldsen, H.
   Korhonen, H.
   Liebig, C.
   Lund, M. N.
   Lundkvist, M.
   Mathiasen, M.
   Penny, M. T.
   Popovas, A.
   Prof, S.
   Rahvar, S.
   Sahu, K.
   Scarpetta, G.
   Schmidt, R. W.
   Schoenebeck, F.
   Snodgrass, C.
   Street, R. A.
   Surdej, J.
   Tsapras, Y.
   Vilela, C.
TI High-precision photometry by telescope defocussing - VI. WASP-24,
   WASP-25 and WASP-26
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: fundamental parameters; planetary systems; stars: individual:
   WASP-24; stars: individual: WASP-25; stars: individual: WASP-26
ID TRANSITING EXTRASOLAR PLANETS; STELLAR EVOLUTION DATABASE;
   PHYSICAL-PROPERTIES; GIANT PLANETS; ECLIPSING BINARIES; STARS; SYSTEM;
   PARAMETERS; RADII; EXOPLANETS
AB We present time series photometric observations of 13 transits in the planetary systems WASP-24, WASP-25 and WASP-26. All three systems have orbital obliquity measurements, WASP-24 andWASP-26 have been observed with Spitzer, andWASP-25 was previously comparatively neglected. Our light curves were obtained using the telescope-defocussing method and have scatters of 0.5-1.2 mmag relative to their best-fitting geometric models. We use these data to measure the physical properties and orbital ephemerides of the systems to high precision, finding that our improved measurements are in good agreement with previous studies. High-resolution Lucky Imaging observations of all three targets show no evidence for faint stars close enough to contaminate our photometry. We confirm the eclipsing nature of the star closest to WASP-24 and present the detection of a detached eclipsing binary within 4.25 arcmin of WASP-26.
C1 [Southworth, John; Hinse, T. C.; Tregloan-Reed, J.; Vilela, C.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
   [Burgdorf, M.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
   [Novati, S. Calchi] HE Space Operat GmbH, D-28199 Bremen, Germany.
   [Novati, S. Calchi; Bozza, V.; D'Ago, G.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy.
   [Novati, S. Calchi; Scarpetta, G.] IIASS, I-84019 Vietri Sul Mare, SA, Italy.
   [Dominik, M.; Galianni, P.; Hundertmark, M.; Browne, P.; Dodds, P.; Jaimes, R. Figuera; Liebig, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
   [Gerner, T.; Giannini, E.; Diehl, C.; Prof, S.; Schmidt, R. W.; Schoenebeck, F.] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
   [Gu, S. -H.; Wang, X. -B.; Fang, X. -S.] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China.
   [Gu, S. -H.; Wang, X. -B.; Fang, X. -S.] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Peoples R China.
   [Jorgensen, U. G.; Juncher, D.; Skottfelt, J.; Andersen, J. M.; Korhonen, H.; Mathiasen, M.; Popovas, A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark.
   [Jorgensen, U. G.; Juncher, D.; Skottfelt, J.; Andersen, J. M.; Hardis, S.; Harpsoe, K.; Korhonen, H.; Mathiasen, M.; Popovas, A.] Univ Copenhagen, Ctr Star & Planet Format, DK-2100 Copenhagen O, Denmark.
   [Kerins, E.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
   [Mancini, L.; Rabus, M.; Ciceri, S.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile.
   [Ricci, D.] Inst Astron UNAM, Ensenada, Baja California, Mexico.
   [Schaefer, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
   [Tregloan-Reed, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Wertz, O.; Damerdji, Y.; Elyiv, A.; Finet, F.; Surdej, J.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
   [Alsubai, K. A.; Bramich, D. M.] Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar.
   [Andersen, J. M.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
   [Bozza, V.; D'Ago, G.; Scarpetta, G.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy.
   [Diehl, C.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany.
   [Elyiv, A.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy.
   [Elyiv, A.] Ukrainian Acad Sci, Main Astron Observ, UA-03680 Kiev, Ukraine.
   [Finet, F.] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, Uttarakhand, India.
   [Jaimes, R. Figuera] European So Observ, D-85748 Garching, Germany.
   [Jessen-Hansen, J.; Kjeldsen, H.; Lund, M. N.; Lundkvist, M.] Aarhus Univ, Dept Phys & Astron, SAC, DK-8000 Aarhus C, Denmark.
   [Kains, N.; Sahu, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Korhonen, H.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland.
   [Penny, M. T.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
   [Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran.
   [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
   [Street, R. A.; Tsapras, Y.] LCOGT, Goleta, CA 93117 USA.
   [Tsapras, Y.] Univ London, Sch Math Sci, London E1 4NS, England.
RP Southworth, J (reprint author), Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
EM astro.js@keele.ac.uk
RI Hundertmark, Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008; Korhonen,
   Heidi/E-3065-2016; D'Ago, Giuseppe/N-8318-2016; 
OI Snodgrass, Colin/0000-0001-9328-2905; Lund, Mikkel
   Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571;
   Hundertmark, Markus/0000-0003-0961-5231; Rahvar,
   Sohrab/0000-0002-7084-5725; Korhonen, Heidi/0000-0003-0529-1161; D'Ago,
   Giuseppe/0000-0001-9697-7331; Dominik, Martin/0000-0002-3202-0343;
   Ricci, Davide/0000-0002-9790-0552
FU Danish Natural Science Research Council; STFC in the form of an Advanced
   Fellowship; European Community [229517, 268421]; Danish National
   Research Foundation; Qatar National Research Fund (a member of Qatar
   Foundation) [NPRP 09-476-1-078, NPRP X-019-1-006]; Korea Research
   Council for Fundamental Science and Technology (KRCF); KASI (Korea
   Astronomy and Space Science Institute) [2012-1-410-02/2013-9-400-00];
   NSFC [10873031]; ASTERISK project (ASTERoseismic Investigations with
   SONG and Kepler) - European Research Council [267864]; Communaute
   francaise de Belgique - Actions de recherche concertees - Academie
   Wallonie-Europe
FX The operation of the Danish 1.54 m telescope is financed by a grant to
   UGJ from the Danish Natural Science Research Council. The reduced light
   curves presented in this work will be made available at the CDS
   (http://vizier.u-strasbg.fr/) and at
   http://www.astro.keele.ac.uk/similar to jkt/. J Southworth acknowledges
   financial support from STFC in the form of an Advanced Fellowship. The
   research leading to these results has received funding from the European
   Community's Seventh Framework Programme (FP7/2007-2013/) under grant
   agreement nos. 229517 and 268421. Funding for the Stellar Astrophysics
   Centre (SAC) is provided by The Danish National Research Foundation.
   This publication was supported by grants NPRP 09-476-1-078 and NPRP
   X-019-1-006 from Qatar National Research Fund (a member of Qatar
   Foundation). TCH acknowledges financial support from the Korea Research
   Council for Fundamental Science and Technology (KRCF) through the Young
   Research Scientist Fellowship Programme and is supported by the KASI
   (Korea Astronomy and Space Science Institute) grant
   2012-1-410-02/2013-9-400-00. SG, XW and XF acknowledge the support from
   NSFC under the grant no. 10873031. The research is supported by the
   ASTERISK project (ASTERoseismic Investigations with SONG and Kepler)
   funded by the European Research Council (grant agreement no. 267864).
   DR, YD, AE, FF (ARC), OW (FNRS research fellow) and J Surdej acknowledge
   support from the Communaute francaise de Belgique - Actions de recherche
   concertees - Academie Wallonie-Europe. The following internet-based
   resources were used in research for this paper: the ESO Digitized Sky
   Survey; the NASA Astrophysics Data System; the SIMBAD data base and
   VizieR catalogue access tool operated at CDS, Strasbourg, France; and
   the arXiv scientific paper preprint service operated by Cornell
   University. We thank the anonymous referee for a helpful report.
NR 57
TC 20
Z9 20
U1 0
U2 5
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 11
PY 2014
VL 444
IS 1
BP 776
EP 789
DI 10.1093/mnras/stu1492
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ6LX
UT WOS:000342925100059
ER

PT J
AU Alatalo, K
   Cales, SL
   Appleton, PN
   Kewley, LJ
   Lacy, M
   Lisenfeld, U
   Nyland, K
   Rich, JA
AF Alatalo, Katherine
   Cales, Sabrina L.
   Appleton, Philip N.
   Kewley, Lisa J.
   Lacy, Mark
   Lisenfeld, Ute
   Nyland, Kristina
   Rich, Jeffrey A.
TI CATCHING QUENCHING GALAXIES: THE NATURE OF THE WISE INFRARED TRANSITION
   ZONE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: evolution; galaxies: ISM; galaxies: star formation; infrared:
   galaxies
ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; STAR-FORMATION; NGC 1266;
   MIDINFRARED SELECTION; HOST GALAXIES; GREEN VALLEY; EMISSION;
   CLASSIFICATION; PARAMETERS
AB We present the discovery of a prominent bifurcation between early-type galaxies and late-type galaxies, in [4.6]-[12] mu m colors from the Wide Field Infrared Survey Explorer (WISE). We then use an emission-line diagnostic comparison sample to explore the nature of objects found both within and near the edges of this WISE infrared transition zone (IRTZ). We hypothesize that this bifurcation might be due to the presence of hot dust and polyaromatic hydrocarbon (PAH) emission features in late-type galaxies. Using a sample of galaxies selected through the Shocked Poststarburst Galaxy Survey (SPOGS), we are able to identify galaxies with strong Balmer absorption (EW(H delta) > 5 angstrom) as well as emission lines inconsistent with star formation (deemed SPOG candidates, or SPOGs*) that lie within the optical green valley. Seyferts and low-ionization nuclear emission line regions, whose u - r colors tend to be red, are strongly represented within IRTZ, whereas SPOGs* tend to sit near the star-forming edge. Although active galactic nuclei are well represented in the IRTZ, we argue that the dominant IRTZ population is composed of galaxies that are in late stages of transitioning across the optical green valley, shedding the last of their remnant interstellar media.
C1 [Alatalo, Katherine; Appleton, Philip N.; Rich, Jeffrey A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
   [Cales, Sabrina L.] Univ Concepcion, Fac Phys & Math Sci, Dept Astron, Concepcion, Chile.
   [Cales, Sabrina L.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA.
   [Appleton, Philip N.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
   [Kewley, Lisa J.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
   [Lacy, Mark] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
   [Lisenfeld, Ute] Univ Granada, Dept Fis Teor & Cosmos, Granada, Spain.
   [Nyland, Kristina] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
   [Nyland, Kristina] Natl Radio Astron Observ, Socorro, NM 87801 USA.
   [Rich, Jeffrey A.] Carnegie Inst Washington Observ, Pasadena, CA 91101 USA.
RP Alatalo, K (reprint author), CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
EM kalatalo@caltech.edu
RI Lisenfeld, Ute/A-1637-2015; 
OI Lisenfeld, Ute/0000-0002-9471-5423; Rich, Jeffrey/0000-0002-5807-5078;
   Appleton, Philip/0000-0002-7607-8766
FU NSF [1109803]; ALMA-CONICYT [31110020]; Spanish Ministerio de Ciencia y
   Educacion [AYA2011-24728]; Junta de Andalucia (Spain) [FQM108]; National
   Aeronautics and Space Administration
FX K.A. thanks Kevin Schawinski for giving full access to his early-and
   late-type galaxy sample, as well as Theodoros Bitsakis and Patrick Ogle
   for insightful discussions, Michelle Cluver and Roc Cutri for WISE
   advice, and finally the referee for an informative and insightful report
   that improved the Letter. K.A. is supported by funding through Herschel,
   a European Space Agency Cornerstone Mission with significant
   participation by NASA, through an award issued by JPL/Caltech. K.N. is
   supported by NSF grant 1109803. S.L.C. was supported by ALMA-CONICYT
   program 31110020. U.L. acknowledges support by the research projects
   AYA2011-24728 from the Spanish Ministerio de Ciencia y Educacion and the
   Junta de Andalucia (Spain) grants FQM108. This publication makes use of
   data products from the Wide-field Infrared Survey Explorer, which is a
   joint project of the University of California, Los Angeles, and the Jet
   Propulsion Laboratory/California Institute of Technology, funded by the
   National Aeronautics and Space Administration. This research has made
   use of the Sloan Digital Sky Survey.<SUP>13</SUP>
NR 45
TC 17
Z9 17
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 OCT 10
PY 2014
VL 794
IS 1
AR L13
DI 10.1088/2041-8205/794/1/L13
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR0YZ
UT WOS:000343304300013
ER

PT J
AU Ingraham, P
   Marley, MS
   Saumon, D
   Marois, C
   Macintosh, B
   Barman, T
   Bauman, B
   Burrows, A
   Chilcote, JK
   De Rosa, RJ
   Dillon, D
   Doyon, R
   Dunn, J
   Erikson, D
   Fitzgerald, MP
   Gavel, D
   Goodsell, SJ
   Graham, JR
   Hartung, M
   Hibon, P
   Kalas, PG
   Konopacky, Q
   Larkin, JA
   Maire, J
   Marchis, F
   McBride, J
   Millar-Blanchaer, M
   Morzinski, KM
   Norton, A
   Oppenheimer, R
   Palmer, DW
   Patience, J
   Perrin, MD
   Poyneer, LA
   Pueyo, L
   Rantakyro, F
   Sadakuni, N
   Saddlemyer, L
   Savransky, D
   Soummer, R
   Sivaramakrishnan, A
   Song, I
   Thomas, S
   Wallace, JK
   Wiktorowicz, SJ
   Wolff, SG
AF Ingraham, Patrick
   Marley, Mark S.
   Saumon, Didier
   Marois, Christian
   Macintosh, Bruce
   Barman, Travis
   Bauman, Brian
   Burrows, Adam
   Chilcote, Jeffrey K.
   De Rosa, Robert J.
   Dillon, Daren
   Doyon, Rene
   Dunn, Jennifer
   Erikson, Darren
   Fitzgerald, Michael P.
   Gavel, Donald
   Goodsell, Stephen J.
   Graham, James R.
   Hartung, Markus
   Hibon, Pascale
   Kalas, Paul G.
   Konopacky, Quinn
   Larkin, James A.
   Maire, Jerome
   Marchis, Franck
   McBride, James
   Millar-Blanchaer, Max
   Morzinski, Katie M.
   Norton, Andrew
   Oppenheimer, Rebecca
   Palmer, Dave W.
   Patience, Jenny
   Perrin, Marshall D.
   Poyneer, Lisa A.
   Pueyo, Laurent
   Rantakyroe, Fredrik
   Sadakuni, Naru
   Saddlemyer, Leslie
   Savransky, Dmitry
   Soummer, Remi
   Sivaramakrishnan, Anand
   Song, Inseok
   Thomas, Sandrine
   Wallace, J. Kent
   Wiktorowicz, Sloane J.
   Wolff, Schuyler G.
TI GEMINI PLANET IMAGER SPECTROSCOPY OF THE HR 8799 PLANETS c AND d
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE infrared: planetary systems; instrumentation: adaptive optics;
   instrumentation: high angular resolution; planets and satellites:
   atmospheres; planets and satellites: gaseous planets; techniques:
   imaging spectroscopy
ID NEAR-INFRARED SPECTROSCOPY; T-DWARFS; 1ST LIGHT; MU-M; ATMOSPHERE;
   CLOUDS; SYSTEM; TRANSITION; MAGNITUDE; MODEL
AB During the first-light run of the Gemini Planet Imager we obtained K-band spectra of exoplanets HR 8799 c and d. Analysis of the spectra indicates that planet d may be warmer than planet c. Comparisons to recent patchy cloud models and previously obtained observations over multiple wavelengths confirm that thick clouds combined with horizontal variation in the cloud cover generally reproduce the planets' spectral energy distributions. When combined with the 3 to 4 mu m photometric data points, the observations provide strong constraints on the atmospheric methane content for both planets. The data also provide further evidence that future modeling efforts must include cloud opacity, possibly including cloud holes, disequilibrium chemistry, and super-solar metallicity.
C1 [Ingraham, Patrick; Macintosh, Bruce] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
   [Marley, Mark S.; Thomas, Sandrine] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Saumon, Didier] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
   [Marois, Christian; Dunn, Jennifer; Erikson, Darren; Saddlemyer, Leslie] NRC Herzberg Astron & Astrophys, Victoria, BC V9E 2E7, Canada.
   [Barman, Travis] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
   [Bauman, Brian; Palmer, Dave W.; Poyneer, Lisa A.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA.
   [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
   [Chilcote, Jeffrey K.; Fitzgerald, Michael P.; Larkin, James A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
   [De Rosa, Robert J.; Patience, Jenny] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
   [De Rosa, Robert J.] Univ Exeter, Coll Engn Math & Phys Sci, Sch Phys, Exeter EX4 4QL, Devon, England.
   [Dillon, Daren; Gavel, Donald; Norton, Andrew; Wiktorowicz, Sloane J.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
   [Doyon, Rene] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
   [Goodsell, Stephen J.; Hartung, Markus; Hibon, Pascale; Rantakyroe, Fredrik; Sadakuni, Naru] Gemini Observ, La Serena, Chile.
   [Graham, James R.; Kalas, Paul G.; McBride, James] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Konopacky, Quinn; Maire, Jerome; Millar-Blanchaer, Max] Univ Toronto, Dunlap Inst Astrophys, Toronto, ON M5S 3H4, Canada.
   [Marchis, Franck] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
   [Morzinski, Katie M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
   [Oppenheimer, Rebecca] Amer Museum Nat Hist, New York, NY 10024 USA.
   [Perrin, Marshall D.; Pueyo, Laurent; Soummer, Remi; Sivaramakrishnan, Anand; Wolff, Schuyler G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Savransky, Dmitry] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA.
   [Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
   [Thomas, Sandrine] Univ Calif Santa Cruz, UARC, Santa Cruz, CA 95064 USA.
   [Wallace, J. Kent] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ingraham, P (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
RI Fitzgerald, Michael/C-2642-2009; Savransky, Dmitry/M-1298-2014; 
OI Fitzgerald, Michael/0000-0002-0176-8973; Savransky,
   Dmitry/0000-0002-8711-7206; Marley, Mark/0000-0002-5251-2943; Morzinski,
   Katie/0000-0002-1384-0063; De Rosa, Robert/0000-0002-4918-0247
FU Gemini; NSF; NASA; U.S. Department of Energy by Lawrence Livermore
   National Laboratory [DE-AC52-07NA27344]
FX The Gemini Observatory is operated by AURA on behalf of the Gemini
   partnership. We acknowledge the financial support of Gemini, NSF, and
   NASA. Portions of this work were performed under the auspices of the
   U.S. Department of Energy by Lawrence Livermore National Laboratory
   under contract DE-AC52-07NA27344. We also thank the large team of
   scientists, engineers, technicians, and others who labored to make GPI a
   reality.
NR 33
TC 17
Z9 17
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 OCT 10
PY 2014
VL 794
IS 1
AR L15
DI 10.1088/2041-8205/794/1/L15
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR0YZ
UT WOS:000343304300015
ER

PT J
AU Kane, SR
   Kopparapu, RK
   Domagal-Goldman, SD
AF Kane, Stephen R.
   Kopparapu, Ravi Kumar
   Domagal-Goldman, Shawn D.
TI ON THE FREQUENCY OF POTENTIAL VENUS ANALOGS FROM KEPLER DATA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrobiology; planetary systems; planets and satellites: individual
   (Venus)
ID MAIN-SEQUENCE STARS; HABITABLE-ZONE; PLANETS; EARTH; MASS; DEPENDENCE;
   RUNAWAY; SYSTEM
AB The field of exoplanetary science has seen a dramatic improvement in sensitivity to terrestrial planets over recent years. Such discoveries have been a key feature of results from the Kepler mission which utilizes the transit method to determine the size of the planet. These discoveries have resulted in a corresponding interest in the topic of the Habitable Zone and the search for potential Earth analogs. Within the solar system, there is a clear dichotomy between Venus and Earth in terms of atmospheric evolution, likely the result of the large difference (approximately a factor of two) in incident flux from the Sun. Since Venus is 95% of the Earth's radius in size, it is impossible to distinguish between these two planets based only on size. In this Letter we discuss planetary insolation in the context of atmospheric erosion and runaway greenhouse limits for planets similar to Venus. We define a "Venus Zone" in which the planet is more likely to be a Venus analog rather than an Earth analog. We identify 43 potential Venus analogs with an occurrence rate (eta female) of 0.32(-0.07)(+0.05) and 0.45(-0.09)(+0.06) for M dwarfs and GK dwarfs, respectively.
C1 [Kane, Stephen R.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA.
   [Kopparapu, Ravi Kumar] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
   [Kopparapu, Ravi Kumar] NASA Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA.
   [Kopparapu, Ravi Kumar] Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA.
   [Kopparapu, Ravi Kumar] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
   [Kopparapu, Ravi Kumar] Blue Marble Space Inst Sci, Seattle, WA 98145 USA.
   [Domagal-Goldman, Shawn D.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kane, SR (reprint author), San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA.
EM skane@sfsu.edu
FU NASA Astrobiology Institute's Virtual Planetary Laboratory lead team;
   NASA [NNH05ZDA001C]
FX We thank the anonymous referee for helpful comments that improved the
   manuscript. The authors thank Eric Lopez and Kevin Zahnle for several
   useful discussions. The authors also thank Courtney Dressing for her
   input in deriving uncertainties on occurrence rates. R.K. gratefully
   acknowledges funding from the NASA Astrobiology Institute's Virtual
   Planetary Laboratory lead team, supported by NASA under cooperative
   agreement NNH05ZDA001C. This work has made use of the Habitable Zone
   Gallery at hzgallery.org.
NR 33
TC 5
Z9 5
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2014
VL 794
IS 1
AR L5
DI 10.1088/2041-8205/794/1/L5
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR0YZ
UT WOS:000343304300005
ER

PT J
AU Ballantyne, DR
   Bollenbacher, JM
   Brenneman, LW
   Madsen, KK
   Balokovic, M
   Boggs, SE
   Christensen, FE
   Craig, WW
   Gandhi, P
   Hailey, CJ
   Harrison, FA
   Lohfink, AM
   Marinucci, A
   Markwardt, CB
   Stern, D
   Walton, DJ
   Zhang, WW
AF Ballantyne, D. R.
   Bollenbacher, J. M.
   Brenneman, L. W.
   Madsen, K. K.
   Balokovic, M.
   Boggs, S. E.
   Christensen, F. E.
   Craig, W. W.
   Gandhi, P.
   Hailey, C. J.
   Harrison, F. A.
   Lohfink, A. M.
   Marinucci, A.
   Markwardt, C. B.
   Stern, D.
   Walton, D. J.
   Zhang, W. W.
TI NuSTAR REVEALS THE COMPTONIZING CORONA OF THE BROAD-LINE RADIO GALAXY 3C
   382
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; galaxies: active; galaxies: individual (3C
   382); galaxies: nuclei; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRA; BLACK-HOLE; SEYFERT-GALAXIES;
   ULTRAVIOLET EXTINCTION; BEPPOSAX OBSERVATIONS; COMPLETE SAMPLE;
   EMISSION-LINES; CYGNUS X-1; IRON LINES
AB Broad-line radio galaxies (BLRGs) are active galactic nuclei that produce powerful, large-scale radio jets, but appear as Seyfert 1 galaxies in their optical spectra. In the X-ray band, BLRGs also appear like Seyfert galaxies, but with flatter spectra and weaker reflection features. One explanation for these properties is that the X-ray continuum is diluted by emission from the jet. Here, we present two NuSTAR observations of the BLRG 3C 382 that show clear evidence that the continuum of this source is dominated by thermal Comptonization, as in Seyfert 1 galaxies. The two observations were separated by over a year and found 3C 382 in different states separated by a factor of 1.7 in flux. The lower flux spectrum has a photon-index of Gamma = 1.68(-0.02)(+0.03), while the photon-index of the higher flux spectrum is Gamma = 1.78(0.03)(+0.02). Thermal and anisotropic Comptonization models provide an excellent fit to both spectra and show that the coronal plasma cooled from kT, = 330 +/- 30 keV in the low flux data to 231(-88)(+50) keV in the high flux observation. This cooling behavior is typical of Comptonizing corona in Seyfert galaxies and is distinct from the variations observed in jet-dominated sources. In the high flux observation, simultaneous Swift data are leveraged to obtain a broadband spectral energy distribution and indicates that the corona intercepts similar to 10% of the optical and ultraviolet emitting accretion disk. 3C 382 exhibits very weak reflection features, with no detectable relativistic Fe Ka line, that may be best explained by an outflowing corona combined with an ionized inner accretion disk.
C1 [Ballantyne, D. R.; Bollenbacher, J. M.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
   [Brenneman, L. W.] Harvard Smithsonian CfA, Cambridge, MA 02138 USA.
   [Madsen, K. K.; Balokovic, M.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
   [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU SpaceNatl Space Inst, DK-2800 Lyngby, Denmark.
   [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
   [Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
   [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Lohfink, A. M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Marinucci, A.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
   [Markwardt, C. B.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ballantyne, DR (reprint author), Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
EM david.ballantync@physics.gatech.edu
RI Boggs, Steven/E-4170-2015
OI Boggs, Steven/0000-0001-9567-4224
FU NASA [NNG0815D60C]; National Aeronautics and Space Administration; NASA
   ADAP grant [NNX13AI47G]; NSF [AST 1008067]; Italian Space Agency
   [ASI/INAF I/037/12/0-011/13]; European Union [312789]; International
   Fulbright Science and Technology Award
FX We thank the referee for a helpful report that improved the paper. This
   work was supported under NASA Contract No. NNG0815D60C, and made use of
   data from the NuSTAR mission, a project led by the California Institute
   of Technology, managed by the Jet Propulsion Laboratory, and funded by
   the National Aeronautics and Space Administration. We thank the NuSTAR
   Operations, Software and Calibration teams for support with the
   execution and analysis of these observations. This research has made use
   of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by
   the ASI Science Data Center (ASDC, Italy) and the California Institute
   of Technology (USA). This work made use of data supplied by the UK Swift
   Science Data Centre at the University of Leicester. 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. D.R.B. acknowledges support from NASA ADAP grant NNX13AI47G
   and NSF award AST 1008067. A.M. acknowledge financial support from
   Italian Space Agency under grant ASI/INAF I/037/12/0-011/13 and from the
   European Union Seventh Framework Programme (FP7/2007-2013) under grant
   agreement n.312789. M.B. acknowledges support from the International
   Fulbright Science and Technology Award.
NR 68
TC 18
Z9 18
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 OCT 10
PY 2014
VL 794
IS 1
AR 62
DI 10.1088/0004-637X/794/1/62
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ1YO
UT WOS:000342581200062
ER

PT J
AU Bayliss, MB
   Ashby, MLN
   Ruel, J
   Brodwin, M
   Aird, KA
   Bautz, MW
   Benson, BA
   Bleem, LE
   Bocquet, S
   Carlstrom, JE
   Chang, CL
   Cho, HM
   Clocchiattii, A
   Crawford, TM
   Crites, AT
   Desai, S
   Dobbs, MA
   Dudley, JP
   Foley, RJ
   Forman, WR
   George, EM
   Gettings, D
   Gladders, MD
   Gonzalez, AH
   de Haan, T
   Halverson, NW
   High, FW
   Holder, GP
   Holzapfel, WL
   Hoover, S
   Hrubes, JD
   Jones, C
   Joy, M
   Keisler, R
   Knox, L
   Lee, AT
   Leitch, EM
   Liu, J
   Lueker, M
   Luong-Van, D
   Mantz, A
   Marrone, DP
   Mawatari, K
   McDonald, M
   McMahon, JJ
   Mehl, J
   Meyer, SS
   Miller, ED
   Mocanu, L
   Mohr, JJ
   Montroy, TE
   Murray, SS
   Padin, S
   Plagge, T
   Pryke, C
   Reichardt, CL
   Rest, A
   Ruhl, JE
   Saliwanchik, BR
   Saro, A
   Sayre, JT
   Schaffer, KK
   Shirokoff, E
   Song, J
   Stalder, B
   Suhada, R
   Spieler, HG
   Stanford, SA
   Staniszewski, Z
   Stark, AA
   Story, K
   Stubbs, CW
   van Engelen, A
   Vanderlinde, K
   Vieira, JD
   Vikhlinin, A
   Williamson, R
   Zahn, R
   Zenteno, A
AF Bayliss, M. B.
   Ashby, M. L. N.
   Ruel, J.
   Brodwin, M.
   Aird, K. A.
   Bautz, M. W.
   Benson, B. A.
   Bleem, L. E.
   Bocquet, S.
   Carlstrom, J. E.
   Chang, C. L.
   Cho, H. M.
   Clocchiattii, A.
   Crawford, T. M.
   Crites, A. T.
   Desai, S.
   Dobbs, M. A.
   Dudley, J. P.
   Foley, R. J.
   Forman, W. R.
   George, E. M.
   Gettings, D.
   Gladders, M. D.
   Gonzalez, A. H.
   de Haan, T.
   Halverson, N. W.
   High, F. W.
   Holder, G. P.
   Holzapfel, W. L.
   Hoover, S.
   Hrubes, J. D.
   Jones, C.
   Joy, M.
   Keisler, R.
   Knox, L.
   Lee, A. T.
   Leitch, E. M.
   Liu, J.
   Lueker, M.
   Luong-Van, D.
   Mantz, A.
   Marrone, D. P.
   Mawatari, K.
   McDonald, M.
   McMahon, J. J.
   Mehl, J.
   Meyer, S. S.
   Miller, E. D.
   Mocanu, L.
   Mohr, J. J.
   Montroy, T. E.
   Murray, S. S.
   Padin, S.
   Plagge, T.
   Pryke, C.
   Reichardt, C. L.
   Rest, A.
   Ruhl, J. E.
   Saliwanchik, B. R.
   Saro, A.
   Sayre, J. T.
   Schaffer, K. K.
   Shirokoff, E.
   Song, J.
   Stalder, B.
   Suhada, R.
   Spieler, H. G.
   Stanford, S. A.
   Staniszewski, Z.
   Stark, A. A.
   Story, K.
   Stubbs, C. W.
   van Engelen, A.
   Vanderlinde, K.
   Vieira, J. D.
   Vikhlinin, A.
   Williamson, R.
   Zahn, R.
   Zenteno, A.
TI SPT-CL J2040-4451: AN SZ-SELECTED GALAXY CLUSTER AT z=1.478 WITH
   SIGNIFICANT ONGOING STAR FORMATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (SPT-CL J2040-4451); galaxies: distances
   and redshifts; galaxies: evolution; large-scale structure of universe
ID SOUTH-POLE TELESCOPE; COLOR-MAGNITUDE RELATION; ZELDOVICH EFFECT SURVEY;
   HIGH-REDSHIFT CLUSTERS; IRAC SHALLOW SURVEY; 720 SQUARE DEGREES;
   GREATER-THAN 1; RED-SEQUENCE; DISTANT CLUSTERS; PHOTOMETRIC REDSHIFTS
AB SPT-CL J2040-4451-spectroscopically confirmed at z = 1.478-is the highest-redshift galaxy cluster yet discovered via the Sunyaev-Zel'dovich effect. SPT-CL J2040-4451 was a candidate galaxy cluster identified in the first 720 deg(2) of the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey, and has been confirmed in follow-up imaging and spectroscopy. From multi-object spectroscopy with Magellan-I/Baade+ IMACS we measure spectroscopic redshifts for 15 cluster member galaxies, all of which have strong [O Pi]lambda lambda 3727 emission. SPT-CL J2040-4451 has an SZ-measured mass of M-500,(SZ) = 3.2 +/- 0.8 x 10(14)M(circle dot) h(-1) 70, corresponding to M-200,M- (SZ) = 5.8 +/- 1.4 x 10(14)M(circle dot) h(70-)(1.) The velocity dispersion measured entirely from blue star-forming members is sv = 1500 +/- 520 km s(-1). The prevalence of star-forming cluster members (galaxies with > 1.5M(circle dot) yr(-1)) implies that this massive, high-redshift cluster is experiencing a phase of active star formation, and supports recent results showing a marked increase in star formation occurring in galaxy clusters at z greater than or similar to 1.4. We also compute the probability of finding a cluster as rare as this in the SPT-SZ survey to be > 99%, indicating that its discovery is not in tension with the concordance Lambda CDM cosmological model.
C1 [Bayliss, M. B.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
   [Bayliss, M. B.; Ashby, M. L. N.; Foley, R. J.; Jones, C.; Mawatari, K.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
   [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA.
   [Bautz, M. W.; Miller, E. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
   [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Keisler, R.; Leitch, E. M.; Mantz, A.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
   [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
   [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
   [Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Mehl, J.] Argonne Natl Lab, Argonne, IL 60439 USA.
   [Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Suhada, R.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
   [Bocquet, S.; Desai, S.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany.
   [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Mocanu, L.; Padin, S.; Plagge, T.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
   [Cho, H. M.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA.
   [Clocchiattii, A.] Pontificia Univ Catolica, Dept Astron & Astrophys, Santiago, Chile.
   [Dobbs, M. A.; Dudley, J. P.; de Haan, T.; Holder, G. P.; van Engelen, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
   [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
   [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
   [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
   [Gettings, D.; Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
   [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
   [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
   [Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA.
   [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
   [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
   [Lueker, M.; Shirokoff, E.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
   [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
   [McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
   [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
   [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA.
   [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
   [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
   [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA.
   [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
   [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
   [Zahn, R.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
   [Zahn, R.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA.
RP Bayliss, MB (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA.
EM mbayliss@cfa.harvard.edu
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; Stubbs,
   Christopher/C-2829-2012; 
OI Williamson, Ross/0000-0002-6945-2975; Stubbs,
   Christopher/0000-0003-0347-1724; Aird, Kenneth/0000-0003-1441-9518;
   Reichardt, Christian/0000-0003-2226-9169; Stark,
   Antony/0000-0002-2718-9996; Forman, William/0000-0002-9478-1682
FU National Science Foundation [ANT-0638937]; NSF Physics Frontier Center
   [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NSF
   [AST-1009012, AST-1009649, MRI-0723073]; National Sciences and
   Engineering Research Council of Canada; Canada Research Chairs program;
   Canadian Institute for Advanced Research; NASA [NAS 8-03060]; Excellence
   Cluster Universe; DFG research program [TR33]; NASA; Clay Fellowship;
   KICP Fellowship; Pennsylvania State University [2834-MIT-SAO-4018];
   Alfred P. Sloan Research Fellowship; Smithsonian Institution; Office of
   Science of the U.S. Department of Energy [DE-AC02-05CH11231]
FX The South Pole Telescope program is supported by the National Science
   Foundation through grant ANT-0638937. Partial support is also provided
   by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli
   Institute of Cosmological Physics at the University of Chicago, the
   Kavli Foundation, and the Gordon and Betty Moore Foundation. Galaxy
   cluster research at Harvard is supported by NSF grant AST-1009012.
   Galaxy cluster research at SAO is supported in part by NSF grants
   AST-1009649 and MRI-0723073. The McGill group acknowledges funding from
   the National Sciences and Engineering Research Council of Canada, Canada
   Research Chairs program, and the Canadian Institute for Advanced
   Research. X-ray research at the CfA is supported through NASA Contract
   NAS 8-03060. The Munich group acknowledges support from the Excellence
   Cluster Universe and the DFG research program TR33. This work is based
   in part on observations obtained with the Spitzer Space Telescope (PID
   60099), 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.
   Additional data were obtained with the 6.5 m Magellan Telescopes located
   at the Las Campanas Observatory, Chile and the Blanco 4 m Telescope at
   Cerro Tololo Interamerican Observatories in Chile. R.J.F. is supported
   by a Clay Fellowship. B.A.B is supported by a KICP Fellowship, M. Bautz
   acknowledges support from contract 2834-MIT-SAO-4018 from the
   Pennsylvania State University to the Massachusetts Institute of
   Technology. M.D. acknowledges support from an Alfred P. Sloan Research
   Fellowship, W.F. and C.J. acknowledge support from the Smithsonian
   Institution. 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. The authors also thank the referee, B. Lemaux, for
   his comments that improved the quality of this paper.
NR 85
TC 19
Z9 19
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 OCT 10
PY 2014
VL 794
IS 1
AR 12
DI 10.1088/0004-637X/794/1/12
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ1YO
UT WOS:000342581200012
ER

PT J
AU Bennett, CJ
   Ennis, CP
   Kaiser, RI
AF Bennett, Chris J.
   Ennis, Courtney P.
   Kaiser, Ralf I.
TI IMPLANTATION OF ENERGETIC D+ IONS INTO CARBON DIOXIDE ICES AND
   IMPLICATIONS FOR OUR SOLAR SYSTEM: FORMATION OF D2O AND D2CO3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; infrared: general; methods: laboratory: solid state;
   molecular processes; planets and satellites: general; radiation
   mechanisms: non-thermal
ID COSMIC-RAY PARTICLES; INTERSTELLAR ICES; ICY SATELLITES; CO2 ICES; 10 K;
   SYMMETRIC ISOMER; MATRIX-ISOLATION; AQUEOUS-SOLUTION; POLAR-REGIONS;
   CONDENSED CO2
AB Carbon dioxide (CO2) ices were irradiated with energetic D+ ions to simulate the exposure of oxygen-bearing solar system ices to energetic protons from the solar wind and magnetospheric sources. The formation of species was observed online and in situ by exploiting FTIR spectroscopy. Molecular products include ozone (O-3), carbon oxides (CO3(C-2v, D-3h), CO4, CO5, CO6), D2-water (D2O), and D2-carbonic acid (D2CO3). Species released into the gas phase were sampled via a quadrupole mass spectrometer, and possible minor contributions from D2-formaldehyde (D2CO), D4-methanol (CD3OD), and D2-formic acid (DCOOD) were additionally identified. The feasibility of several reaction networks was investigated by determining their ability to fit the observed temporal column densities of 10 key species that were quantified during the irradiation period. Directly relevant to the CO2-bearing ices of comets, icy satellites in the outer solar system, and the ice caps on Mars, this work illustrates for the first time that D2-water is formed as a product of the exposure of CO2 ices to D+ ions. These findings provide strong support for water formation from oxygen-bearing materials via non-thermal hydrogen atoms, and predict reaction pathways that are likely to be unfolding on the surfaces of asteroids and the Moon.
C1 [Bennett, Chris J.; Ennis, Courtney P.; Kaiser, Ralf I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA.
   [Bennett, Chris J.; Kaiser, Ralf I.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
   [Bennett, Chris J.; Kaiser, Ralf I.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
RP Bennett, CJ (reprint author), Georgia Inst Technol, 901 Atlantic Dr, Atlanta, GA 30332 USA.
EM ralfk@hawaii.edu
RI Ennis, Courtney/M-5050-2015; 
OI Ennis, Courtney/0000-0003-1774-8982; Bennett,
   Christopher/0000-0002-4181-6976
FU National Aeronautics and Space Administration (NASA Astrobiology
   Institute) through the Office of Space Science [NNA09DA77A]
FX This material was based upon work supported by the National Aeronautics
   and Space Administration (NASA Astrobiology Institute under Cooperative
   Agreement No. NNA09DA77A issued through the Office of Space Science).
NR 97
TC 3
Z9 3
U1 1
U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2014
VL 794
IS 1
AR 57
DI 10.1088/0004-637X/794/1/57
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ1YO
UT WOS:000342581200057
ER

PT J
AU Carpenter, KG
   Ayres, TR
   Harper, GM
   Kober, G
   Nielsen, KE
   Wahlgren, GM
AF Carpenter, Kenneth G.
   Ayres, Thomas R.
   Harper, Graham M.
   Kober, Gladys
   Nielsen, Krister E.
   Wahlgren, Glenn M.
TI AN HST COS "SNAPSHOT" SPECTRUM OF THE K SUPERGIANT lambda Vel (K4Ib-II)*
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: atmospheres; stars: chromospheres; stars individual (lambda Vel,
   alpha Boo, alpha On); stars: late-type; stars: mass-loss; supergiants
ID LOW-GRAVITY STARS; ZETA-AURIGAE; EMISSION-LINES; ALPHA-ORIONIS;
   EFFECTIVE TEMPERATURES; ULTRAVIOLET-SPECTRUM; ANGULAR DIAMETERS; GHRS
   OBSERVATIONS; ARCTURUS; WIND
AB We present a far-ultraviolet spectrum of the K4 lb-II supergiant Vel obtained with the Hubble Space Telescope's Cosmic Origins Spectrograph (COS) as a part of the SN, APshot program "SNAPing coronal iron" (GO 11687). The observation covers a wavelength region (1326-1467 angstrom) not previously recorded for Vel at a spectral resolving power of R similar to 20,000 and displays strong emission and absorption features, superposed on a bright chromospheric continuum. Fluorescent excitation is responsible for much of the observed emission, mainly powered by strong Hi Ly alpha and the 0 (UV 2) triplet emission near),1304. The molecular CO and H-2 fluorescences are weaker than in the early-K giant alpha Boo while the Fell and Cr II lines, also pumped by HI Ly alpha, are stronger in lambda Vel. This pattern of relative line strengths between the two stars is explained by the lower iron-group element abundance in a Boo, which weakens that star's Fell and Cr II emission without reducing the molecular fluorescences. The lambda Vel spectrum shows fluorescent Fe ii, Cr ii, and H-2 emission similar to that observed in the M supergiant alpha Ori, but more numerous well-defined narrow emissions from CO. The additional CO emissions are visible in the spectrum of Vel since that star does not have the cool, opaque circumstellar shells that surround a On and produce broad circumstellar CO (A-X) band absorptions that hide those emissions in the cooler star. The presence of Si w emission in Vel indicates a similar to 8 x 10(4) K plasma that is mixed into the cooler chromosphere. Evidence of the stellar wind is seen in the C)1334,1335 lines and in the blueshifted Fe II and Ni ii wind absorption lines. Line modeling using Sobolev with Exact Integration for the C ii lines indicates a larger terminal velocity (similar to 45 versus similar to 30 km s(-1)) and turbulence (similar to 27 versus <21 km s(-1)) with a more quickly accelerating wind (t = 0.35 versus 0.7) at the time of this COS observation in 2010 than derived from Goddard High Resolution Spectrograph data obtained in 1994. The Fe ii and Ni ii absorptions are blueshifted by 7.6 km s(-1) relative to the chromospheric emission, suggesting formation in lower levels of the accelerating wind and their widths indicate a higher turbulence in the Vel wind compared to a On.
C1 [Carpenter, Kenneth G.] NASA, Greenbelt, MD 20771 USA.
   [Ayres, Thomas R.] Univ Colorado, CASA, Boulder, CO 80309 USA.
   [Harper, Graham M.] Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland.
   [Kober, Gladys; Nielsen, Krister E.; Wahlgren, Glenn M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Carpenter, KG (reprint author), NASA, GSFC Code 667, Greenbelt, MD 20771 USA.
EM Kenneth.G.Carpenter@nasa.gov
FU NASA through grants from the Space Telescope Science Institute
   [GO-11687, GO-12278]; NASA [NAS5-26555]
FX Support for GO-11687 and GO-12278 was provided by NASA through grants
   from the Space Telescope Science Institute, which is operated by the
   Association of Universities for Research in Astronomy, Inc., under NASA
   contract NAS5-26555.
NR 46
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2014
VL 794
IS 1
AR 41
DI 10.1088/0004-637X/794/1/41
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ1YO
UT WOS:000342581200041
ER

PT J
AU Dolch, T
   Lam, MT
   Cordes, J
   Chatterjee, S
   Bassa, C
   Bhattacharyya, B
   Champion, DJ
   Cognard, I
   Crowter, K
   Demorest, PB
   Hessels, JWT
   Janssen, G
   Jenet, FA
   Jones, G
   Jordan, C
   Karuppusamy, R
   Keith, M
   Kondratiev, V
   Kramer, M
   Lazarus, P
   Lazio, TJW
   Lee, KJ
   McLaughlin, MA
   Roy, J
   Shannon, RM
   Stairs, I
   Stovall, K
   Verbiest, JPW
   Madison, DR
   Palliyaguru, N
   Perrodin, D
   Ransom, S
   Stappers, B
   Zhu, WW
   Dai, S
   Desvignes, G
   Guillemot, L
   Liu, K
   Lyne, A
   Perera, BBP
   Petroff, E
   Rankin, JM
   Smits, R
AF Dolch, T.
   Lam, M. T.
   Cordes, J.
   Chatterjee, S.
   Bassa, C.
   Bhattacharyya, B.
   Champion, D. J.
   Cognard, I.
   Crowter, K.
   Demorest, P. B.
   Hessels, J. W. T.
   Janssen, G.
   Jenet, F. A.
   Jones, G.
   Jordan, C.
   Karuppusamy, R.
   Keith, M.
   Kondratiev, V.
   Kramer, M.
   Lazarus, P.
   Lazio, T. J. W.
   Lee, K. J.
   McLaughlin, M. A.
   Roy, J.
   Shannon, R. M.
   Stairs, I.
   Stovall, K.
   Verbiest, J. P. W.
   Madison, D. R.
   Palliyaguru, N.
   Perrodin, D.
   Ransom, S.
   Stappers, B.
   Zhu, W. W.
   Dai, S.
   Desvignes, G.
   Guillemot, L.
   Liu, K.
   Lyne, A.
   Perera, B. B. P.
   Petroff, E.
   Rankin, J. M.
   Smits, R.
TI A 24 HR GLOBAL CAMPAIGN TO ASSESS PRECISION TIMING OF THE MILLISECOND
   PULSAR J1713+0747
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational waves; ISM: structure; pulsars: individual (PSR
   J1713+0747)
ID GRAVITATIONAL-WAVE MEMORY; INTERSTELLAR SCINTILLATION; BINARY-SYSTEMS;
   RADIO PULSARS; ARRAY; LIMITS; BAND; LOFAR; PSR-B1534+12; STATISTICS
AB The radio millisecond pulsar J1713+0747 is regarded as one of the highest-precision clocks in the sky and is regularly timed for the purpose of detecting gravitational waves. The International Pulsar Timing Array Collaboration undertook a 24 hr global observation of PSR J1713+0747 in an effort to better quantify sources of timing noise in this pulsar, particularly on intermediate (1-24 hr) timescales. We observed the pulsar continuously over 24 hr with the Arecibo, Effelsberg, GMRT, Green Bank, LOFAR, Lovell, Nancay, Parkes, and WSRT radio telescopes. The combined pulse times-of-arrival presented here provide an estimate of what sources of timing noise, excluding DM variations, would be present as compared to an idealized,root N improvement in timing precision, where N is the number of pulses analyzed. In the case of this particular pulsar, we find that intrinsic pulse phase jitter dominates arrival time precision when the signal-to-noise ratio of single pulses exceeds unity, as measured using the eight telescopes that observed at L band/1.4 GHz. We present first results of specific phenomena probed on the unusually long timescale (for a single continuous observing session) of tens of hours, in particular interstellar scintillation, and discuss the degree to which scintillation and profile evolution affect precision timing. This paper presents the data set as a basis for future, deeper studies.
C1 [Dolch, T.; Lam, M. T.; Cordes, J.; Chatterjee, S.; Madison, D. R.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
   [Dolch, T.] Oberlin Coll, Oberlin, OH 44074 USA.
   [Bassa, C.; Hessels, J. W. T.; Janssen, G.; Kondratiev, V.; Smits, R.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands.
   [Bassa, C.; Bhattacharyya, B.; Janssen, G.; Jordan, C.; Keith, M.; Roy, J.; Stappers, B.; Lyne, A.; Perera, B. B. P.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
   [Bhattacharyya, B.; Roy, J.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
   [Champion, D. J.; Karuppusamy, R.; Kramer, M.; Lazarus, P.; Lee, K. J.; Verbiest, J. P. W.; Desvignes, G.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
   [Cognard, I.; Guillemot, L.; Liu, K.] LPC2E UMR 6115 CNRS, Lab Phys & Chim Environm & Espace, F-45071 Orleans 02, France.
   [Cognard, I.; Guillemot, L.; Liu, K.] Observ Paris, CNRS INSU, Stn Radioastron Nancay, F-18330 Nancay, France.
   [Crowter, K.; Stairs, I.; Zhu, W. W.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
   [Demorest, P. B.; Ransom, S.] Natl Radio Astron Observ, Charlottesville, VA 22901 USA.
   [Hessels, J. W. T.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
   [Jenet, F. A.] Univ Texas Brownsville, Ctr Adv Radio Astron, Brownsville, TX 78520 USA.
   [Jones, G.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Kondratiev, V.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia.
   [Kramer, M.] Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England.
   [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
   [Lee, K. J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
   [McLaughlin, M. A.] Univ Virginia, Dept Phys & Astron, Morgantown, WV 26506 USA.
   [Shannon, R. M.; Dai, S.; Petroff, E.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
   [Stovall, K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
   [Verbiest, J. P. W.] Univ Bielefeld, Dept Phys, D-33501 Bielefeld, Germany.
   [Perrodin, D.] INAF Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy.
   [Dai, S.] Peking Univ, Sch Phys, Beijing 100871, Peoples R China.
   [Petroff, E.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
   [Petroff, E.] Swinburne Univ Technol, ARC Ctr Excellence All Sky Astrophys CAASTRO, Hawthorn, Vic 3122, Australia.
   [Rankin, J. M.] Univ Vermont, Dept Phys, Burlington, VT 05401 USA.
RP Dolch, T (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
EM tdolch@astro.cornell.edu
RI Perrodin, Delphine/L-1916-2016; 
OI Perrodin, Delphine/0000-0002-1806-2483; Ransom,
   Scott/0000-0001-5799-9714
FU National Science Foundation (NSF) PIRE program award [0968296]; IMPRS
   Bonn/Cologne; FQRNT B2; NSERC; Canadian Institute for Advanced Research;
   STFC rolling grant; Region Centre in France; Commonwealth of Australia;
   ERC [227947]; National Aeronautics and Space Administration; ERC
   Starting Grant "DRAGNET" [337062]
FX The work of S.J.C., J.M.C., P.B.D., T.D., F.J., G.J., M.T.L., T.J.W.L.,
   J.L., D.R.M., M.A.M., N.P., S.M.R., and K.S. was partially supported
   through the National Science Foundation (NSF) PIRE program award number
   0968296. P.L. acknowledges the support of IMPRS Bonn/Cologne and FQRNT
   B2. We thank the telescope schedulers Hector Hernandez, Alex Kraus, Tony
   Minter, and many others for working hard to ensure that this observation
   was given adequate time, given the difficulty of scheduling nine
   telescopes for simultaneous observations. We thank the staff of the GMRT
   who have made these observations possible. The GMRT is run by the
   National Centre for Radio Astrophysics of the Tata Institute of
   Fundamental Research. NANOGrav research at University of British
   Columbia is supported by an NSERC Discovery Grant and Discovery
   Accelerator Supplement and by the Canadian Institute for Advanced
   Research. 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. The 100 m Effelsberg telescope is operated by the
   Max-Planck-Institut fur Radioastronomie (MPIfR). 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. Access to the Lovell Telescope is supported through an STFC
   rolling grant. The Nancay radio telescope is part of the Paris
   Observatory, associated with the Centre National de la Recherche
   Scientifique (CNRS), and partially supported by the Region Centre in
   France. The Parkes Radio telescope is part of the Australia Telescope
   National Facility which is funded by the Commonwealth of Australia for
   operation as a National Facility managed by CSIRO. The Westerbork
   Synthesis Radio Telescope is operated by the Netherlands Foundation for
   Research in Astronomy (ASTRON) with support from the NWO (Netherlands
   Organisation for Scientific Research). Some of this work was supported
   by the ERC Advanced Grant "LEAP," Grant Agreement Number 227947 (PI: M.
   Kramer). 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. Analysis of LOFAR
   data was supported by ERC Starting Grant "DRAGNET" (337062; PI: J.
   Hessels).
NR 78
TC 16
Z9 17
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 OCT 10
PY 2014
VL 794
IS 1
AR 21
DI 10.1088/0004637X/794/1/21
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ1YO
UT WOS:000342581200021
ER

PT J
AU Gicquel, A
   Milam, SN
   Villanueva, GL
   Remijan, AJ
   Coulson, IM
   Chuang, YL
   Charnley, SB
   Cordiner, MA
   Kuan, YJ
AF Gicquel, A.
   Milam, S. N.
   Villanueva, G. L.
   Remijan, A. J.
   Coulson, I. M.
   Chuang, Y. -L.
   Charnley, S. B.
   Cordiner, M. A.
   Kuan, Y. -J.
TI GROUND-BASED MULTIWAVELENGTH OBSERVATIONS OF COMET 103P/HARTLEY 2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; comets: individual (103P/Hartley2); radio lines: planetary
   systems; submillimeter: planetary systems; techniques: spectroscopic
ID O1 HALE-BOPP; NUCLEAR-SPIN CONVERSION; SPITZER-SPACE-TELESCOPE; EPOXI
   CLOSEST APPROACH; JUPITER-FAMILY COMETS; C/2001 Q4 NEAT; WATER
   PRODUCTION; DEEP IMPACT; ROTATIONAL TEMPERATURE; CHEMICAL-COMPOSITION
AB The Jupiter-family comet 103P/Hartley 2 (103P) was the target of the NASA EPOXI mission. In support of this mission, we conducted observations from radio to submillimeter wavelengths of comet 103P in the three weeks preceding the spacecraft rendezvous onUT2010 November 4.58. This time period included the passage at perihelion and the closest approach of the comet to the Earth. Here, we report detections of HCN, H2CO, CS, and OH and upper limits for HNC and DCN toward 103P using the Arizona Radio Observatory Kitt Peak 12 m telescope (ARO 12 m) and submillimeter telescope (SMT), the James ClerkMaxwell Telescope (JCMT), and the Green Bank Telescope (GBT). The water production rate, Q(H2O) = (0.67-1.07) x 10(28) s(-1), was determined from the GBT OH data. From the average abundance ratios of HCN and H2CO relative to water (0.13 +/- 0.03% and 0.14 +/- 0.03%, respectively), we conclude that H2CO is depleted and HCN is normal with respect to typically observed cometary mixing ratios. However, the abundance ratio of HCN with water shows a large diversity with time. Using the JCMT data, we measured an upper limit for the DCN/HCN ratio < 0.01. Consecutive observations of ortho-H2CO and para-H2CO on November 2 (from data obtained at the JCMT) allowed us to derive an ortho: para ratio (OPR) of approximate to 2.12 +/- 0.59 (1 sigma), corresponding to T-spin > 8 K (2 sigma).
C1 [Gicquel, A.; Villanueva, G. L.; Cordiner, M. A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
   [Gicquel, A.; Milam, S. N.; Villanueva, G. L.; Charnley, S. B.; Cordiner, M. A.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
   [Remijan, A. J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
   [Coulson, I. M.] Joint Astron Ctr, Hilo, HI 96720 USA.
   [Chuang, Y. -L.; Kuan, Y. -J.] Natl Taiwan Normal Univ, Taipei 116, Taiwan.
   [Kuan, Y. -J.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
RP Gicquel, A (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave NE, Washington, DC 20064 USA.
EM adeline.gicquel@nasa.gov; stelanie.n.milam@nasa.gov;
   geronimo.l.villanueva@nasa.gov; aremijan@nrao.edu;
   i.coulson@jach.hawaii.edu; ylchuang@std.ntnu.edu.tw;
   steven.b.charnley@nasa.gov; martin.a.cordiner@nasa.gov; kuan@ntnu.edu.tw
RI Milam, Stefanie/D-1092-2012
OI Milam, Stefanie/0000-0001-7694-4129
FU Goddard Center for Astrobiology; NASA's Planetary Astronomy Program;
   NASA's Planetary Atmospheres Program; NSC [100-2119-M-003-001-MY3,
   102-2119-M-003-008-]
FX The National Radio Astronomy Observatory is a facility of the National
   Science Foundation operated under cooperative agreement by Associated
   Universities, Inc. The Kitt Peak 12 m telescope and the Submillimeter
   telescope are currently operated by the Arizona Observatory (ARO),
   Steward Observatory, University of Arizona, with partial funding from
   the Research Corporation. The James Clerk Maxwell Telescope is operated
   by the Joint Astronomy Centre on behalf of the Science and Technology
   Facilities Council of the United Kingdom, the Netherlands Organisation
   for Scientific Research, and the National Research Council of Canada.
   This work was supported by the Goddard Center for Astrobiology, by
   NASA's Planetary Astronomy and Planetary Atmospheres Programs. Y.J.K.
   acknowledges support from NSC grants 100-2119-M-003-001-MY3 and
   102-2119-M-003-008- for this work.
NR 78
TC 5
Z9 5
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2014
VL 794
IS 1
AR 1
DI 10.1088/0004-637X/794/1/1
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ1YO
UT WOS:000342581200001
ER

PT J
AU Howard, AW
   Marcy, GW
   Fischer, DA
   Isaacson, H
   Muirhead, PS
   Henry, GW
   Boyajian, TS
   Von Braun, K
   Becker, JC
   Wright, JT
   Johnson, JA
AF Howard, Andrew W.
   Marcy, Geoffrey W.
   Fischer, Debra A.
   Isaacson, Howard
   Muirhead, Philip S.
   Henry, Gregory W.
   Boyajian, Tabetha S.
   Von Braun, Kaspar
   Becker, Juliette C.
   Wright, Jason T.
   Johnson, John Asher
TI THE NASA-UC-UH ETA-EARTH PROGRAM. IV. A LOW-MASS PLANET ORBITING AN M
   DWARF 3.6 PC FROM EARTH
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (Gliese 15 A); techniques: radial
   velocities
ID EXOPLANET HOST STARS; EXTRA-SOLAR PLANETS; K-BAND SPECTRA; SUN-LIKE
   STARS; SUPER-EARTH; ASTROPHYSICAL PARAMETERS; HABITABLE ZONE; HARPS
   SEARCH; TRANSITING PLANET; CHARA ARRAY
AB We report the discovery of a low-mass planet orbiting Gl 15A based on radial velocities from the Eta-Earth Survey using HIRES at Keck Observatory. Gl 15 Ab is a planet with minimum mass M sin i = 5.35 +/- 0.75M(circle plus), orbital period P = 11.4433 +/- 0.0016 days, and an orbit that is consistent with circular. We characterize the host star using a variety of techniques. Photometric observations at Fairborn Observatory show no evidence for rotational modulation of spots at the orbital period to a limit of similar to 0.1 mmag, thus supporting the existence of the planet. We detect a second RV signal with a period of 44 days that we attribute to rotational modulation of stellar surface features, as confirmed by optical photometry and the Ca II H & K activity indicator. Using infrared spectroscopy from Palomar-TripleSpec, we measure an M2 V spectral type and a sub-solar metallicity ([M/H] = -0.22, [Fe/H] = -0.32). We measure a stellar radius of 0.3863 +/- 0.0021R(circle dot) based on interferometry from CHARA.
C1 [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
   [Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Fischer, Debra A.; Boyajian, Tabetha S.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
   [Muirhead, Philip S.; Becker, Juliette C.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
   [Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA.
   [Von Braun, Kaspar] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
   [Von Braun, Kaspar] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Wright, Jason T.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
   [Wright, Jason T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
   [Johnson, John Asher] CALTECH, Ctr Planetary Astron, Pasadena, CA 91125 USA.
RP Howard, AW (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
RI Howard, Andrew/D-4148-2015; Muirhead, Philip/H-2273-2014; 
OI Howard, Andrew/0000-0001-8638-0320; Muirhead,
   Philip/0000-0002-0638-8822; Wright, Jason/0000-0001-6160-5888; Becker,
   Juliette/0000-0002-7733-4522
FU NASA grant [NNX12AJ23G]; NASA; NSF; Tennessee State University; State of
   Tennessee through Centers of Excellence program; David & Lucile Packard
   Foundation; Alfred P. Sloan Foundation
FX We thank the many observers who contributed to the measurements reported
   here. We gratefully acknowledge the efforts and dedication of the Keck
   Observatory staff, especially Scott Dahm, Greg Doppman, Hien Tran, and
   Grant Hill for support of HIRES and Greg Wirth for support of remote
   observing. We thank Kevin Apps, Andrew Mann, Evan Sinukoff, and Calla
   Howard for helpful discussions. We are grateful to the time assignment
   committees of the University of Hawaii, the University of California,
   and NASA for their generous allocations of observing time. Without their
   long-term commitment to RV monitoring, this planet would likely remain
   unknown. We acknowledge R. Paul Butler and S.S. Vogt for many years of
   contributing to the data presented here. A.W.H. acknowledges NASA grant
   NNX12AJ23G. G.W.H. acknowledges support from NASA, NSF, Tennessee State
   University, and the State of Tennessee through its Centers of Excellence
   program. J.A.J. gratefully acknowledges support from generous grants
   from the David & Lucile Packard and Alfred P. Sloan Foundations. This
   work made use of the SIMBAD database (operated at CDS, Strasbourg,
   France), NASA's Astrophysics Data System Bibliographic Services, and the
   NASA Star and Exoplanet Database (NStED). Finally, the authors wish to
   extend special thanks to those of Hawai'ian ancestry on whose sacred
   mountain of Mauna Kea we are privileged to be guests. Without their
   generous hospitality, the Keck observations presented herein would not
   have been possible.
NR 103
TC 24
Z9 24
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 OCT 10
PY 2014
VL 794
IS 1
AR 51
DI 10.1088/0004-637X/794/1/51
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ1YO
UT WOS:000342581200051
ER

PT J
AU Johnson, JA
   Huber, D
   Boyajian, T
   Brewer, JM
   White, TR
   von Braun, K
   Maestro, V
   Stello, D
   Barclay, T
AF Johnson, John Asher
   Huber, Daniel
   Boyajian, Tabetha
   Brewer, John M.
   White, Timothy R.
   von Braun, Kaspar
   Maestro, Vicente
   Stello, Dennis
   Barclay, Thomas
TI THE PHYSICAL PARAMETERS OF THE RETIRED A STAR HD 185351
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: abundances; stars: individual (HD 185351); stars: interiors;
   stars: oscillations
ID SOLAR-LIKE OSCILLATIONS; STELLAR ASTROPHYSICS MESA; BASE-LINE
   INTERFEROMETRY; VIRTUAL OBSERVATORY TOOL; GIANT IOTA-DRACONIS; SUN-LIKE
   STAR; K-TYPE STARS; RED-GIANT; CHARA ARRAY; MAIN-SEQUENCE
AB We report here an analysis of the physical stellar parameters of the giant star HD 185351 using Kepler short-cadence photometry, optical and near infrared interferometry from CHARA, and high-resolution spectroscopy. Asteroseismic oscillations detected in the Kepler short-cadence photometry combined with an effective temperature calculated from the interferometric angular diameter and bolometric flux yield a mean density rho(star) = 0.0130 +/- 0.0003 rho(circle dot) and surface gravity log g = 3.280+/-0.011. Combining the gravity and density we find R-star = 5.35 +/- 0.20 R-circle dot and M-star=1.99 +/- 0.23M(circle dot). The trigonometric parallax and CHARA angular diameter give a radius R-star = 4.97+/-0.07 R-circle dot. This smaller radius, when combined with the mean stellar density, corresponds to a stellar mass 1.60 +/- 0.08 M-circle dot, which is smaller than the asteroseismic mass by 1.6 sigma. We find that a larger mass is supported by the observation of mixed modes in our high-precision photometry, the spacing of which is consistent only for M-star greater than or similar to 1.8M(circle dot). Our various and independent mass measurements can be compared to the mass measured from interpolating the spectroscopic parameters onto stellar evolution models, which yields a model-based mass M-star, (model) = 1.87+/-0.07 M-circle dot. This mass agrees well with the asteroseismic value, but is 2.6 sigma higher than the mass from the combination of asteroseismology and interferometry. The discrepancy motivates future studies with a larger sample of giant stars. However, all of our mass measurements are consistent with HD 185351 having a mass in excess of 1.5M(circle dot).
C1 [Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
   [Huber, Daniel; Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA.
   [Boyajian, Tabetha; Brewer, John M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
   [White, Timothy R.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
   [White, Timothy R.; Maestro, Vicente; Stello, Dennis] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia.
   [von Braun, Kaspar] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Stello, Dennis] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
   [Barclay, Thomas] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
RP Johnson, JA (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
OI Brewer, John/0000-0002-9873-1471; Boyajian, Tabetha/0000-0001-9879-9313
FU NASA Science Mission directorate; NASA [NAS5-26555, NNX14AB92G,
   ADAP12-0172]; NASA Office of Space Science [NNX09AF08G]; W.M. Keck
   Foundation; Alfred P. Sloan foundation; David and Lucile Packard
   foundation; National Science Foundation [AST-0606958, AST-0908253];
   Georgia State University through the College of Arts and Sciences; W. M.
   Keck Foundation; Danish National Research Foundation [DNRF106]; ASTERISK
   project (ASTERoseismic Investigations with SONG and Kepler) - European
   Research Council [267864]
FX This paper includes data collected by the Kepler mission. Funding for
   the Kepler mission is provided by the NASA Science Mission directorate.
   We are grateful to the Kepler Team for their extensive efforts in
   producing such high quality data. Some of the data presented in this
   paper were obtained from the Multimission Archive at the Space Telescope
   Science Institute (MAST). STScI is operated by the Association of
   Universities for Research in Astronomy, Inc., under NASA contract
   NAS5-26555. Support for MAST for non-HST data is provided by the NASA
   Office of Space Science via grant NNX09AF08G and by other grants and
   contracts.; 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. We gratefully acknowledge the efforts and dedication of the
   Keck Observatory staff, especially Grant Hill and Scott Dahm for support
   of HIRES and Greg Wirth for support of remote observing. The authors
   wish to recognize and acknowledge the very significant cultural role and
   reverence that the summit of Mauna Kea has always had within the
   indigenous Hawaiian community. We are most fortunate to have the
   opportunity to conduct observations from this mountain.; J.A.J. is
   grateful for the generous grant support provided by the Alfred P. Sloan
   and David and Lucile Packard foundations, and acknowledges enlightening
   conversations with Dimitar Sasselov, Peter Goldreich, Phil Muirhead,
   Jason Wright, Debra Fischer, Jeff Valenti, James Lloyd and Victoria
   "Ashley" Villar.; D.H. acknowledges support by an appointment to the
   NASA Postdoctoral Program at Ames Research Center administered by Oak
   Ridge Associated Universities, and NASA Grant NNX14AB92G issued through
   the Kepler Participating Scientist Program.; T.S.B acknowledges support
   provided through NASA grant ADAP12-0172.; The CHARA Array is funded by
   the National Science Foundation through NSF grants AST-0606958 and
   AST-0908253 and by Georgia State University through the College of Arts
   and Sciences, as well as the W. M. Keck Foundation.; Funding for the
   Stellar Astrophysics Centre is provided by The Danish National Research
   Foundation (grant agreement No.: DNRF106). The research is supported by
   the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler)
   funded by the European Research Council (grant agreement No.: 267864).
NR 133
TC 16
Z9 16
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2014
VL 794
IS 1
AR 15
DI 10.1088/0004-637X/794/1/15
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ1YO
UT WOS:000342581200015
ER

PT J
AU Luo, B
   Brandt, WN
   Alexander, DM
   Stern, D
   Teng, SH
   Arevalo, P
   Bauer, FE
   Boggs, SE
   Christensen, FE
   Comastri, A
   Craig, WW
   Farrah, D
   Gandhi, P
   Hailey, CJ
   Harrison, FA
   Koss, M
   Ogle, P
   Puccetti, S
   Saez, C
   Scott, AE
   Walton, DJ
   Zhang, WW
AF Luo, B.
   Brandt, W. N.
   Alexander, D. M.
   Stern, D.
   Teng, S. H.
   Arevalo, P.
   Bauer, F. E.
   Boggs, S. E.
   Christensen, F. E.
   Comastri, A.
   Craig, W. W.
   Farrah, D.
   Gandhi, P.
   Hailey, C. J.
   Harrison, F. A.
   Koss, M.
   Ogle, P.
   Puccetti, S.
   Saez, C.
   Scott, A. E.
   Walton, D. J.
   Zhang, W. W.
TI WEAK HARD X-RAY EMISSION FROM BROAD ABSORPTION LINE QUASARS: EVIDENCE
   FOR INTRINSIC X-RAY WEAKNESS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; galaxies: active; galaxies: nuclei; quasars:
   absorption lines; quasars: emission lines; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; DRIVEN DISK WINDS; STELLAR
   OBJECTS; DATA RELEASE; SEYFERT-GALAXIES; ULTRAVIOLET EXTINCTION; NUSTAR
   OBSERVATIONS; INFRARED GALAXIES; CONFIDENCE-LIMITS
AB We report NuSTAR observations of a sample of six X-ray weak broad absorption line (BAL) quasars. These targets, at z = 0.148-1.223, are among the optically brightest and most luminous BAL quasars known at z < 1.3. However, their rest-frame approximate to 2 keV luminosities are 14 to >330 times weaker than expected for typical quasars. Our results from a pilot NuSTAR study of two low-redshift BAL quasars, a Chandra stacking analysis of a sample of highredshift BAL quasars, and a NuSTAR spectral analysis of the local BAL quasar Mrk 231 have already suggested the existence of intrinsically X-ray weak BAL quasars, i.e., quasars not emitting X-rays at the level expected from their optical/UV emission. The aim of the current program is to extend the search for such extraordinary objects. Three of the six new targets are weakly detected by NuSTAR with <= 45 counts in the 3-24 keV band, and the other three are not detected. The hard X-ray (8-24 keV) weakness observed by NuSTAR requires Compton-thick absorption if these objects have nominal underlying X-ray emission. However, a soft stacked effective photon index (Gamma(eff) approximate to 1.8) for this sample disfavors Compton-thick absorption in general. The uniform hard X-ray weakness observed by NuSTAR for this and the pilot samples selected with <10 keV weakness also suggests that the X-ray weakness is intrinsic in at least some of the targets. We conclude that the NuSTAR observations have likely discovered a significant population (>= 33%) of intrinsically X-ray weak objects among the BAL quasars with significantly weak <10 keV emission. We suggest that intrinsically X-ray weak quasars might be preferentially observed as BAL quasars.
C1 [Luo, B.; Brandt, W. N.; Scott, A. E.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
   [Luo, B.; Brandt, W. N.; Scott, A. E.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
   [Alexander, D. M.; Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
   [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Teng, S. H.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Arevalo, P.; Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
   [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso 1111, Chile.
   [Bauer, F. E.] Millennium Inst Astrophys, Santiago 7820436, Chile.
   [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
   [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Christensen, F. E.] Tech Univ Denmark, DTU SpaceNat Space Inst, DK-2800 Lyngby, Denmark.
   [Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
   [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
   [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
   [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
   [Koss, M.] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
   [Ogle, P.] CALTECH, IPAC, Pasadena, CA 91125 USA.
   [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy.
   [Puccetti, S.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy.
   [Saez, C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Luo, B (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt,
   William/N-2844-2015; Comastri, Andrea/O-9543-2015; 
OI Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581;
   Brandt, William/0000-0002-0167-2453; Comastri,
   Andrea/0000-0003-3451-9970; Puccetti, Simonetta/0000-0002-2734-7835
FU California Institute of Technology (Caltech) NuSTAR [44A-1092750]; NASA
   ADP grant [NNX1OAC99G]; NASA [NNG081-D60C]; CONICYT-Chile FONDECYT
   [1140304, 1141218]; "EMBIGGEN" Anillo [ACT1101]; Basal-CATA
   [PFB-06/2007]; "Millennium Institute of Astrophysics (MAS)" of
   Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y
   Turismo [IC120009]; ASI/INAF [I/037/12/0-011/13]; STFC [ST/J003697/1];
   Swiss National Science Foundation (NSF) [PP00P2 138979/1]
FX We acknowledge support from the California Institute of Technology
   (Caltech) NuSTAR subcontract 44A-1092750 (B.L., W.N.B.), NASA ADP grant
   NNX1OAC99G (B.L., W.N.B.), NASA Postdoctoral Program (S.H.T.),
   CONICYT-Chile FONDECYT 1140304 (P.A.) and 1141218 (F.E.B.), "EMBIGGEN"
   Anillo ACT1101 (P.A., F.E.B.), Basal-CATA PFB-06/2007 (F.E.B.), Project
   IC120009 "Millennium Institute of Astrophysics (MAS)" of Iniciativa
   Cientifica Milenio del Ministerio de Economia, Fomento y Turismo
   (F.E.B.), ASI/INAF grant I/037/12/0-011/13 (A.C.), STFC grant
   ST/J003697/1 (P.G.), and the Swiss National Science Foundation (NSF)
   grant PP00P2 138979/1 (M.K.). We thank K. Forster for help with the
   observation planning, and we thank T. Yaqoob for helpful discussions. We
   thank the referee for carefully reviewing the manuscript and providing
   helpful comments. This work was supported under NASA Contract No.
   NNG081-D60C, and made use of data from the NuSTAR mission, a project led
   by Caltech, 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 NuSTAR-DAS jointly developed by the ASI Science Data Center (ASDC,
   Italy) and Caltech (USA).
NR 91
TC 20
Z9 20
U1 1
U2 11
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 OCT 10
PY 2014
VL 794
IS 1
AR 70
DI 10.1088/0004-637X/794/1/70
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ1YO
UT WOS:000342581200070
ER

PT J
AU Provornikova, E
   Opher, M
   Izmodenov, VV
   Richardson, JD
   Toth, G
AF Provornikova, E.
   Opher, M.
   Izmodenov, V. V.
   Richardson, J. D.
   Toth, G.
TI PLASMA FLOWS IN THE HELIOSHEATH ALONG THE VOYAGER 1 AND 2 TRAJECTORIES
   DUE TO EFFECTS OF THE 11 YR SOLAR CYCLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE interplanetary medium; magnetohydrodynamics (MHD); solar wind; Sun:
   activity; Sun: heliosphere
ID INTERSTELLAR MAGNETIC-FIELD; OUTER HELIOSPHERE; 3-DIMENSIONAL FEATURES;
   DYNAMICAL HELIOSPHERE; TERMINATION SHOCK; TRANSITION REGION; WIND;
   MODEL; BOUNDARY; VELOCITY
AB We investigate the role of the 11 yr solar cycle variations in the solar wind (SW) parameters on the flows in the heliosheath using a new three-dimensional time-dependent model of the interaction between the SW and the interstellar medium. For boundary conditions in the model we use realistic time and the latitudinal dependence of the SW parameters obtained from SOHO/SWAN and interplanetary scintillation data for the last two solar cycles (1990-2011). This data set generally agrees with the in situ Ulysses measurements from 1991 to 2009. For the first similar to 30AU of the heliosheath the time-dependent model predicts constant radial flow speeds at Voyager 2 (V2), which is consistent with observations and different from the steady models that show a radial speed decrease of 30%. The model shows that V2 was immersed in SW with speeds of 500-550 km s(-1) upstream of the termination shock before 2009 and in wind with upstream speeds of 450-500 km s(-1) after 2009. The model also predicts that the radial velocity along the Voyager 1 (V1) trajectory is constant across the heliosheath, contrary to observations. This difference in observations implies that additional effects may be responsible for the different flows at V1 and V2. The model predicts meridional flows (VN) higher than those observed because of the strong bluntness of the heliosphere shape in the N direction in the model. The modeled tangential velocity component (VT) at V2 is smaller than observed. Both VN and VT essentially depend on the shape of the heliopause.
C1 [Provornikova, E.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
   [Provornikova, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Provornikova, E.; Izmodenov, V. V.] RAS, Space Res Inst, Moscow 117997, Russia.
   [Opher, M.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
   [Izmodenov, V. V.] Moscow MV Lomonosov State Univ, Moscow 119991, Russia.
   [Izmodenov, V. V.] Inst Problems Mech, Moscow 119526, Russia.
   [Richardson, J. D.] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA.
   [Toth, G.] Univ Michigan, Ann Arbor, MI 48109 USA.
RP Provornikova, E (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
EM elena.a.provornikova@nasa.gov; mopher@bu.edu; izmod@iki.rssi.ru;
   jdr@space.mit.edu; gtoth@umich.odu
RI Toth, Gabor/B-7977-2013; Izmodenov, Vladislav/K-6073-2012
OI Toth, Gabor/0000-0002-5654-9823; Izmodenov,
   Vladislav/0000-0002-1748-0982
FU NSF CAREER Grant [ATM-0747654]; RFBR [14-02-00746]; NASA Voyager project
   through JPL; NASA [NNX13AE04G]
FX This research benefited from discussions at the meetings of the
   Heliopause Team at the ISSI in Bern, Switzerland. We thank O. Katushkina
   for providing us with the SW data set at 1 AU and for useful
   discussions. These data are based on SOHO/SWAN, OMNI database, and IPS
   results. IPS data analysis was performed by J. Sokol and M. Bzowski.
   Analysis of the SOHO/SWAN maps was carried out by the SOHO/SWAN team. We
   thank Robert Decker for providing us with the data on plasma flows
   derived from LECP/Voyager 1 measurements for comparison with our model
   results. This work was supported by NSF CAREER Grant ATM-0747654. The
   calculations were performed with the NASA AMES Pleiades Supercomputer.
   V.I. and E.P. acknowledge partial support by RFBR grant 14-02-00746.
   J.D.R. was supported by the NASA Voyager project through JPL. M.O. was
   supported by NASA grant NNX13AE04G.
NR 36
TC 7
Z9 7
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 OCT 10
PY 2014
VL 794
IS 1
AR 29
DI 10.1088/0004-637X/794/1/29
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ1YO
UT WOS:000342581200029
ER

PT J
AU Wagstaff, KL
   Thompson, DR
   Bue, BD
   Fuchs, TJ
AF Wagstaff, Kiri L.
   Thompson, David R.
   Bue, Brian D.
   Fuchs, Thomas J.
TI AUTONOMOUS REAL-TIME DE ILCTION OF PLUMES AND JETS FROM MOONS AND COMETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets: general; methods: data analysis; planets and satellites:
   general; techniques: image processing
ID 103P/HARTLEY 2; ENCELADUS; EPOXI; SPACECRAFT; ONBOARD; CAMERA; EO-1
AB Dynamic activity on the surface of distant moons, asteroids, and comets can manifest as jets or plumes. These phenomena provide information about the interior of the bodies and the forces (gravitation, radiation, thermal) they experience. Fast detection and follow-up study is imperative since the phenomena may be time-varying and because the observing window may be limited (e.g., during a flyby). We have developed an advanced method for real-time detection of plumes and jets using onboard analysis of the data as it is collected. In contrast to prior work, our technique is not restricted to plume detection from spherical bodies, making it relevant for irregularly shaped bodies such as comets. Further, our study analyzes raw data, the form in which it is available on board the spacecraft, rather than fully processed image products. In summary, we contribute a vital assessment of a technique that can be used on board tomorrow's deep space missions to detect, and respond quickly to, new occurrences of plumes and jets.
C1 [Wagstaff, Kiri L.; Thompson, David R.; Bue, Brian D.; Fuchs, Thomas J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wagstaff, KL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kiri.l.wagstaff@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX We gratefully acknowledge the Planetary Data System (PDS) for providing
   the Cassini and Deep Impact data used in this study. We thank Kenneth
   Klaasen for his assistance with the Deep Impact images of comet Hartley
   2. This work was carried out at the Jet Propulsion Laboratory,
   California Institute of Technology, under a contract with the National
   Aeronautics and Space Administration. Government sponsorship
   acknowledged. Copyright 2014, California Institute of Technology.
NR 30
TC 4
Z9 4
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2014
VL 794
IS 1
AR 43
DI 10.1088/0004-637X/794/1/43
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ1YO
UT WOS:000342581200043
ER

PT J
AU Muniyan, S
   Chou, YW
   Ingersoll, MA
   Devine, A
   Morris, M
   Odero-Marah, VA
   Khan, SA
   Chaney, WG
   Bu, XR
   Lin, MF
AF Muniyan, Sakthivel
   Chou, Yu-Wei
   Ingersoll, Matthew A.
   Devine, Alexus
   Morris, Marisha
   Odero-Marah, Valerie A.
   Khan, Shafiq A.
   Chaney, William G.
   Bu, Xiu R.
   Lin, Ming-Fong
TI Antiproliferative activity of novel imidazopyridine derivatives on
   castration-resistant human prostate cancer cells
SO CANCER LETTERS
LA English
DT Article
DE Prostate cancer; Imidazopyridine; Androgen receptor; PI3K/Akt; p66Shc
ID TUMOR-SUPPRESSOR P53; ACID-PHOSPHATASE; IN-VIVO; TYROSINE
   PHOSPHORYLATION; P66(SHC) PROTEIN; BAX GENE; BCL-XL; ANDROGEN;
   INHIBITOR; EXPRESSION
AB Metastatic prostate cancer (mPCa) relapses after a short period of androgen deprivation therapy and becomes the castration-resistant prostate cancer (CR PCa); to which the treatment is limited. Hence, it is imperative to identify novel therapeutic agents towards this patient population. In the present study, antiproliferative activities of novel imidazopyridines were compared. Among three derivatives, PHE, AMD and AMN, examined, AMD showed the highest inhibitory activity on LNCaP C-81 cell proliferation, following dose- and time-dependent manner. Additionally, AMD exhibited significant antiproliferative effect against a panel of PCa cells, but not normal prostate epithelial cells. Further, when compared to AMD, its derivative DME showed higher inhibitory activities on PCa cell proliferation, clonogenic potential and in vitro tumorigenicity. The inhibitory activity was apparently in part due to the induction of apoptosis. Mechanistic studies indicate that AMD and DME treatments inhibited both AR and PI3K/Akt signaling. The results suggest that better understanding of inhibitory mechanisms of AMD and DME could help design novel therapeutic agents for improving the treatment of CR PCa. (C) 2014 Elsevier Ireland Ltd. All rights reserved.
C1 [Muniyan, Sakthivel; Chou, Yu-Wei; Ingersoll, Matthew A.; Chaney, William G.; Lin, Ming-Fong] Univ Nebraska, Med Ctr, Dept Biochem & Mol Biol, Omaha, NE 68198 USA.
   [Chou, Yu-Wei] Kaohsiung Chang Gung Mem Hosp, Kaohsiung, Taiwan.
   [Devine, Alexus; Bu, Xiu R.] Clark Atlanta Univ, Dept Chem, Atlanta, GA 30314 USA.
   [Morris, Marisha; Odero-Marah, Valerie A.; Khan, Shafiq A.] Clark Atlanta Univ, Dept Biol Sci, Atlanta, GA 30314 USA.
   [Odero-Marah, Valerie A.; Khan, Shafiq A.] Clark Atlanta Univ, Ctr Canc Res & Therapeut Dev, Atlanta, GA 30314 USA.
   [Bu, Xiu R.] Clark Atlanta Univ, Lab Electroopt Mat, Atlanta, GA 30314 USA.
   [Bu, Xiu R.] Clark Atlanta Univ, NASA, Ctr High Performance Polymers & Composites, Atlanta, GA 30314 USA.
   [Lin, Ming-Fong] Univ Nebraska, Med Ctr, Eppley Inst Res Canc & Allied Dis, Omaha, NE 68198 USA.
   [Lin, Ming-Fong] Univ Nebraska, Med Ctr, Dept Urol Surg, Omaha, NE 68198 USA.
   [Lin, Ming-Fong] Kaohsiung Med Univ, Sch Pharm, Kaohsiung 807, Taiwan.
RP Lin, MF (reprint author), Univ Nebraska, Med Ctr, Coll Med, Dept Biochem & Mol Biol, 985870 Nebraska Med Ctr, Omaha, NE 68198 USA.
EM mlin@unmc.edu
OI Muniyan, Sakthivel/0000-0001-9405-7857
FU National Cancer Institute, National Institutes of Health [R01 CA88184];
   Department of Defense PCa Training Grant [PC094594, PC121645];
   University of Nebraska Medical Center Bridge Fund
FX This work was supported in part by the National Cancer Institute,
   National Institutes of Health [R01 CA88184]; Department of Defense PCa
   Training Grant [PC094594, PC121645]; and the University of Nebraska
   Medical Center Bridge Fund.
NR 50
TC 11
Z9 11
U1 1
U2 10
PU ELSEVIER IRELAND LTD
PI CLARE
PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000,
   IRELAND
SN 0304-3835
EI 1872-7980
J9 CANCER LETT
JI Cancer Lett.
PD OCT 10
PY 2014
VL 353
IS 1
BP 59
EP 67
DI 10.1016/j.canlet.2014.07.002
PG 9
WC Oncology
SC Oncology
GA AP7PI
UT WOS:000342268800008
PM 25050738
ER

PT J
AU Mazaheri, A
   Nishikawa, H
AF Mazaheri, Alireza
   Nishikawa, Hiroaki
TI Very efficient high-order hyperbolic schemes for time-dependent
   advection-diffusion problems: Third-, fourth-, and sixth-order
SO COMPUTERS & FLUIDS
LA English
DT Article
DE Higher-order; Residual distribution; Unsteady; Nonlinear; Navier-Stokes
ID RESIDUAL DISTRIBUTION SCHEMES; STEADY; MESHES
AB In this paper, we construct very efficient high-order schemes for general time-dependent advection-diffusion problems, based on the first-order hyperbolic system method. Extending the previous work on the second-order time-dependent hyperbolic advection-diffusion scheme (Mazaheri and Nishikawa, NASA/TM-2014-218175, 2014), we construct third-, fourth-, and sixth-order accurate schemes by modifying the source term discretization. In this paper, two techniques for the source term discretization are proposed; (I) reformulation of the source terms with their divergence forms and (2) correction to the trapezoidal rule for the source term discretization. We construct spatially third- and fourth-order schemes from the former technique. These schemes require computations of the gradients and second-derivatives of the source terms. From the latter technique, we construct spatially third-, fourth-, and sixth-order schemes by using the gradients and second-derivatives for the source terms, except the fourth-order scheme, which does not require the second derivatives of the source term and thus is even less computationally expensive than the third-order schemes. We then construct high-order time-accurate schemes by incorporating a high-order backward difference formula as a source term. These schemes are very efficient in that high-order accuracy is achieved for both the solution and the gradient only by the improved source term discretization. A very rapid Newton-type convergence is achieved by a compact second-order Jacobian formulation. The numerical results are presented for both steady and time-dependent linear and nonlinear advection-diffusion problems, demonstrating these powerful features. Published by Elsevier Ltd.
C1 [Mazaheri, Alireza] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Nishikawa, Hiroaki] NIA, Hampton, VA 23666 USA.
RP Mazaheri, A (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM ali.r.mazaheri@nasa.gov
RI Nishikawa, Hiroaki/M-1247-2016
OI Nishikawa, Hiroaki/0000-0003-4472-5313
FU U.S. Army Research Office [W911NF-12-1-0154]
FX The second author is supported by the U.S. Army Research Office under
   the Contract/Grant Number W911NF-12-1-0154.
NR 24
TC 7
Z9 7
U1 0
U2 4
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 OCT 10
PY 2014
VL 102
BP 131
EP 147
DI 10.1016/j.compfluid.2014.06.020
PG 17
WC Computer Science, Interdisciplinary Applications; Mechanics
SC Computer Science; Mechanics
GA AP7RL
UT WOS:000342274300013
ER

PT J
AU Bachetti, M
   Harrison, FA
   Walton, DJ
   Grefenstette, BW
   Chakrabarty, D
   Furst, F
   Barret, D
   Beloborodov, A
   Boggs, SE
   Christensen, FE
   Craig, WW
   Fabian, AC
   Hailey, CJ
   Hornschemeier, A
   Kaspi, V
   Kulkarni, SR
   Maccarone, T
   Miller, JM
   Rana, V
   Stern, D
   Tendulkar, SP
   Tomsick, J
   Webb, NA
   Zhang, WW
AF Bachetti, M.
   Harrison, F. A.
   Walton, D. J.
   Grefenstette, B. W.
   Chakrabarty, D.
   Fuerst, F.
   Barret, D.
   Beloborodov, A.
   Boggs, S. E.
   Christensen, F. E.
   Craig, W. W.
   Fabian, A. C.
   Hailey, C. J.
   Hornschemeier, A.
   Kaspi, V.
   Kulkarni, S. R.
   Maccarone, T.
   Miller, J. M.
   Rana, V.
   Stern, D.
   Tendulkar, S. P.
   Tomsick, J.
   Webb, N. A.
   Zhang, W. W.
TI An ultraluminous X-ray source powered by an accreting neutron star
SO NATURE
LA English
DT Article
ID STRONG MAGNETIC-FIELD; XMM-NEWTON; GALAXY M82; DISCOVERY; PULSARS;
   CHANDRA; PULSATIONS; RADIATION; MODELS; SYSTEM
AB The majority of ultraluminous X-ray sources are point sources that are spatially offset from the nuclei of nearby galaxies and whose X-ray luminosities exceed the theoretical maximum for spherical infall (the Eddington limit) onto stellar-mass black holes(1,2). Their X-ray luminosities in the 0.5-10 kiloelectronvolt energy band range from 10(39) to 10(41) ergs per second(3). Because higher masses imply less extreme ratios of the luminosity to the isotropic Eddington limit, theoretical models have focused on black hole rather than neutron star systems(1,2). The most challenging sources to explain are those at the luminous end of the range (more than 10(40) ergs per second), which require black hole masses of 50-100 times the solar value or significant departures from the standard thin disk accretion that powers bright Galactic X-ray binaries, or both. Here we report broadband X-ray observations of the nuclear region of the galaxy M82 that reveal pulsations with an average period of 1.37 seconds and a 2.5-day sinusoidal modulation. The pulsations result from the rotation of a magnetized neutron star, and the modulation arises from its binary orbit. The pulsed flux alone corresponds to an X-ray luminosity in the 3-30 kiloelectronvolt range of 4.9 x 10(39) ergs per second. The pulsating source is spatially coincident with a variable source(4) that can reach an X-ray luminosity in the 0.3-10 kiloelectronvolt range of 1.8 x 10(40) ergs per second(1). This association implies a luminosity of about 100 times the Eddington limit for a 1.4-solar-mass object, or more than ten times brighter than any known accreting pulsar. This implies that neutron stars may not be rare in the ultraluminous X-ray population, and it challenges physical models for the accretion of matter onto magnetized compact objects.
C1 [Bachetti, M.; Barret, D.; Webb, N. A.] Univ Toulouse, UPS OMP, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France.
   [Bachetti, M.; Barret, D.; Webb, N. A.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France.
   [Harrison, F. A.; Walton, D. J.; Grefenstette, B. W.; Fuerst, F.; Kulkarni, S. R.; Rana, V.; Tendulkar, S. P.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
   [Chakrabarty, D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
   [Beloborodov, A.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
   [Boggs, S. E.; Tomsick, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
   [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
   [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
   [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Hornschemeier, A.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Kaspi, V.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
   [Maccarone, T.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA.
   [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
   [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bachetti, M (reprint author), Univ Toulouse, UPS OMP, Inst Rech Astrophys & Planetol, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France.
EM mbachett@oa-cagliari.inaf.it; fiona@srl.caltech.edu
RI Boggs, Steven/E-4170-2015; 
OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337
FU NASA [NNG08FD60C]; NASA; Centre National d'Etudes Spatiales (CNES);
   Centre National de la Recherche Scientifique (CNRS)
FX This work was supported by NASA (grant no. NNG08FD60C), and made use of
   data from the Nuclear Spectroscopic Telescope Array (NuSTAR) mission, a
   project led by Caltech, managed by the Jet Propulsion Laboratory and
   funded by NASA. We thank the NuSTAR operations, software and calibration
   teams for support with execution and analysis of these observations.
   This work made use of data supplied by the UK Swift Science Data Centre
   at the University of Leicester. M.B. thanks the Centre National d'Etudes
   Spatiales (CNES) and the Centre National de la Recherche Scientifique
   (CNRS) for support. Line plots were done using Veusz software by J.
   Sanders.
NR 34
TC 111
Z9 111
U1 3
U2 14
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 OCT 9
PY 2014
VL 514
IS 7521
BP 202
EP +
DI 10.1038/nature13791
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AQ3BG
UT WOS:000342663100036
PM 25297433
ER

PT J
AU Carvalhais, N
   Forkel, M
   Khomik, M
   Bellarby, J
   Jung, M
   Migliavacca, M
   Mu, MQ
   Saatchi, S
   Santoro, M
   Thurner, M
   Weber, U
   Ahrens, B
   Beer, C
   Cescatti, A
   Randerson, JT
   Reichstein, M
AF Carvalhais, Nuno
   Forkel, Matthias
   Khomik, Myroslava
   Bellarby, Jessica
   Jung, Martin
   Migliavacca, Mirco
   Mu, Mingquan
   Saatchi, Sassan
   Santoro, Maurizio
   Thurner, Martin
   Weber, Ulrich
   Ahrens, Bernhard
   Beer, Christian
   Cescatti, Alessandro
   Randerson, James T.
   Reichstein, Markus
TI Global covariation of carbon turnover times with climate in terrestrial
   ecosystems
SO NATURE
LA English
DT Article
ID SOIL ORGANIC-CARBON; VEGETATION MODEL; ATMOSPHERIC CO2; RESPIRATION;
   TEMPERATURE; DYNAMICS; PRODUCTIVITY; MATTER; STOCK; PRECIPITATION
AB The response of the terrestrial carbon cycle to climate change is among the largest uncertainties affecting future climate change projections(1,2). The feedback between the terrestrial carbon cycle and climate is partly determined by changes in the turnover time of carbon in land ecosystems, which in turn is an ecosystem property that emerges from the interplay between climate, soil and vegetation type(3-6). Here we present a global, spatially explicit and observation-based assessment of whole-ecosystem carbon turnover times that combines new estimates of vegetation and soil organic carbon stocks and fluxes. We find that the overall mean global carbon turnover time is 23(4)(+7) years (95 per cent confidence interval). Onaverage, carbon resides in the vegetation and soil near the Equator for a shorter time than at latitudes north of 75 degrees north (mean turnover times of 15 and 255 years, respectively). We identify a clear dependence of the turnover time on temperature, as expected from our present understanding of temperature controls on ecosystem dynamics. Surprisingly, our analysis also reveals a similarly strong association between turnover time and precipitation. Moreover, we find that the ecosystem carbon turnover times simulated by state-of-the-art coupled climate/carbon-cycle models vary widely and that numerical simulations, on average, tend to underestimate the global carbon turnover time by 36 per cent. The models show stronger spatial relationships with temperature than do observation-based estimates, but generally do not reproduce the strong relationships with precipitation and predict faster carbon turnover in many semiarid regions. Our findings suggest that future climate/carbon-cycle feedbacks may depend more strongly on changes in the hydrological cycle than is expected at present and is considered in Earth system models.
C1 [Carvalhais, Nuno; Forkel, Matthias; Khomik, Myroslava; Jung, Martin; Migliavacca, Mirco; Thurner, Martin; Weber, Ulrich; Ahrens, Bernhard; Beer, Christian; Reichstein, Markus] Max Planck Inst Biogeochem, D-07745 Jena, Germany.
   [Carvalhais, Nuno] Univ Nova Lisboa, FCT, DCEA, P-2829516 Caparica, Portugal.
   [Khomik, Myroslava] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON L8S 4K1, Canada.
   [Bellarby, Jessica] Univ Aberdeen, Sch Biol Sci, Inst Biol & Environm Sci, Aberdeen AB24 3UU, Scotland.
   [Bellarby, Jessica] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England.
   [Migliavacca, Mirco] Univ Milano Bicocca, DISAT, Remote Sensing Environm Dynam Lab, I-20126 Milan, Italy.
   [Mu, Mingquan; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
   [Saatchi, Sassan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Santoro, Maurizio] Gamma Remote Sensing, CH-3073 Gumlingen, Switzerland.
   [Beer, Christian] Stockholm Univ, Dept Appl Environm Sci, S-10691 Stockholm, Sweden.
   [Beer, Christian] Stockholm Univ, Bolin Ctr Climate Res, S-10691 Stockholm, Sweden.
   [Cescatti, Alessandro] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, Climate Risk Management Unit, I-21027 Ispra, Italy.
RP Carvalhais, N (reprint author), Max Planck Inst Biogeochem, Hans Knoll Str 10, D-07745 Jena, Germany.
EM nuno.carvalhais@bgc-jena.mpg.de
RI Beer, Christian/D-2296-2013
FU European Union (FP7) through the project GEOCARBON [283080]; ERC
   starting grant QUASOM [ERC-2007-StG-208516]; European Union (FP7)
   through the project CARBONES [242316]; European Union (FP7) through the
   project EMBRACE [283201]
FX We would like to thank C. Jones for comments that improved the
   manuscript. We are grateful to A. Ito, D. Zaks and S. Del Grosso for
   sharing their NPP data sets with us. We thank S. Schott for figure
   editing. We acknowledge support by the European Union (FP7) through the
   projects GEOCARBON (283080), CARBONES (242316) and EMBRACE (283201) and
   an ERC starting grant QUASOM (ERC-2007-StG-208516).
NR 71
TC 88
Z9 90
U1 62
U2 300
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 OCT 9
PY 2014
VL 514
IS 7521
BP 213
EP +
DI 10.1038/nature13731
PG 17
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AQ3BG
UT WOS:000342663100039
PM 25252980
ER

PT J
AU Yoonessi, M
   Lebron-Colon, M
   Scheiman, D
   Meador, MA
AF Yoonessi, Mitra
   Lebron-Colon, Marisabel
   Scheiman, Daniel
   Meador, Michael A.
TI Carbon Nanotube Epoxy Nanocomposites: The Effects of Interfacial
   Modifications on the Dynamic Mechanical Properties of the Nanocomposites
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE carbon nanotube; epoxy; polymer nanocomposites; surface
   functionalization
ID LARGE-SCALE SYNTHESIS; DAMPING CHARACTERISTICS; POLYMER NANOCOMPOSITES;
   SINGLE-WALL; REINFORCED COMPOSITES; ELECTRON-MICROSCOPY; POLYIMIDE;
   FUNCTIONALIZATION; SILANIZATION; DISPERSIONS
AB Surface functionalization of pretreated carbon nanotubes (CNT) using aromatic, aliphatic, and aliphatic ether diamines was performed. The pretreatment of the CNT consisted of either acid- or photo-oxidation. The acid treated CNT had a higher initial oxygen content compared to the photo-oxidized CNT and this resulted in a higher density of functionalization. X-ray photoelectron spectroscopy (XPS) and thermal gravimetric analysis (TGA) were used to verify the presence of the oxygenated and amine moieties on the CNT surfaces. Epoxy/0.1 wt % CNT nanocomposites were prepared using the functionalized CNT and the bulk properties of the nanocomposites were examined. Macroscale correlations between the interfacial modification and bulk dynamic mechanical and thermal properties were observed. The amine modified epoxy/CNT nanocomposites exhibited up to a 1.9-fold improvement in storage modulus (G') below the glass transition (T-g) and up to an almost 4-fold increase above the T-g. They also exhibited a 3-10 degrees C increase in the glass transition temperature. The aromatic diamine surface modified epoxy/CNT nanocomposites resulted in the largest increase in shear moduli below and above the T-g and the largest increase in the T-g. Surface examination of the nanocomposites with scanning electron microscopy (SEM) revealed indications of a greater adhesion of the epoxy resin matrix to the CNT, most likely due to the covalent bonding.
C1 [Yoonessi, Mitra] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
   [Lebron-Colon, Marisabel; Meador, Michael A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
   [Scheiman, Daniel] ASRC, Cleveland, OH 44135 USA.
RP Yoonessi, M (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.
EM mitra.yoonessi@gmai.com
FU NASA Aeronautics-Subsonic Fixed Wing Program [NNC07BA13B]
FX The NASA Aeronautics-Subsonic Fixed Wing Program (Contract NNC07BA13B)
   provided financial support for this work. NASA summer faculty fellowship
   program and Dr. Kankam are thanked. Ms. Dorothy Lokco and Dave Hull are
   thanked for their support for XPS, HR-TEM, and FE-SEM.
NR 47
TC 21
Z9 22
U1 5
U2 91
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 OCT 8
PY 2014
VL 6
IS 19
BP 16621
EP 16630
DI 10.1021/am5056849
PG 10
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA AQ7RZ
UT WOS:000343018200020
PM 25215892
ER

PT J
AU Vo, T
   von Allmen, P
   Huang, CK
   Ma, J
   Bux, S
   Fleurial, JP
AF Trinh Vo
   von Allmen, Paul
   Huang, Chen-Kuo
   Ma, James
   Bux, Sabah
   Fleurial, Jean-Pierre
TI Electronic and thermoelectric properties of Ce3Te4 and La3Te4 computed
   with density functional theory with on-site Coulomb interaction
   correction
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID YB14MNSB11; NANOWIRES; FIGURE; MERIT; TE
AB The electronic properties and Seebeck coefficients of Ce3Te4 and La3Te4 are computed using Density Functional Theory with on-site Coulomb interaction correction. We found that the Seebeck coefficients of Ce3Te4 and La3Te4 are almost equal at temperatures larger than the Curie temperature of Ce3Te4, and in good agreement with the measurements reported by May et al. [Phys. Rev. B 86, 035135 (2012)]. At temperatures below the Curie temperature, the Seebeck coefficient of Ce3Te4 increases due to the ferromagnetic ordering, which leads the f-electron of Ce to contribute to the Seebeck coefficient in the relevant range of electron concentration. (C) 2014 AIP Publishing LLC.
C1 [Trinh Vo; von Allmen, Paul; Huang, Chen-Kuo; Ma, James; Bux, Sabah; Fleurial, Jean-Pierre] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Vo, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU National Aeronautics and Space Administration; NASA Science Mission
   Directorate's Radioisotope Power Systems Technology Advancement Program
FX This work was performed at the Jet Propulsion Laboratory, California
   Institute of Technology under contract with the National Aeronautics and
   Space Administration. This work was supported by the NASA Science
   Mission Directorate's Radioisotope Power Systems Technology Advancement
   Program.
NR 28
TC 1
Z9 1
U1 3
U2 16
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
   MELVILLE, NY 11747-4501 USA
SN 0021-8979
EI 1089-7550
J9 J APPL PHYS
JI J. Appl. Phys.
PD OCT 7
PY 2014
VL 116
IS 13
AR 133701
DI 10.1063/1.4896670
PG 6
WC Physics, Applied
SC Physics
GA AR9DQ
UT WOS:000343872500029
ER

PT J
AU Fleddermann, R
   Ward, RL
   Elliot, M
   Wuchenich, DM
   Gilles, F
   Herding, M
   Nicklaus, K
   Brown, J
   Burke, J
   Dligatch, S
   Farrant, DI
   Green, KL
   Seckold, JA
   Blundell, M
   Brister, R
   Smith, C
   Sheard, BS
   Heinzel, G
   Danzmann, K
   Klipstein, B
   McClelland, DE
   Shaddock, DA
AF Fleddermann, R.
   Ward, R. L.
   Elliot, M.
   Wuchenich, D. M.
   Gilles, F.
   Herding, M.
   Nicklaus, K.
   Brown, J.
   Burke, J.
   Dligatch, S.
   Farrant, D. I.
   Green, K. L.
   Seckold, J. A.
   Blundell, M.
   Brister, R.
   Smith, C.
   Sheard, B. S.
   Heinzel, G.
   Danzmann, K.
   Klipstein, B.
   McClelland, D. E.
   Shaddock, D. A.
TI Testing the GRACE follow-on triple mirror assembly
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
DE gravity recovery and climate explorer; GRACE; triple mirror assembly;
   laser ranging instrument; GRACE follow-on; retroreflectors; coalignment
   measurements
AB We report on the successful testing of the GRACE follow-on triple mirror assembly (TMA) prototype. This component serves to route the laser beam in a proposed follow-on mission to the Gravity Recovery and Climate Explorer (GRACE) mission, containing an optical instrument for space-based distance measurement between satellites. As part of this, the TMA has to meet a set of stringent requirements on both the optical and mechanical properties. The purpose of the TMA prototype testing is to establish the feasibility of the design, materials choice and fabrication techniques. Here we report on co-alignment testing of this device to the arc second (5 mu rad) level and thermal alignment stability testing to 1 mu rad K-1.
C1 [Fleddermann, R.; Ward, R. L.; Elliot, M.; Wuchenich, D. M.; McClelland, D. E.; Shaddock, D. A.] Australian Natl Univ, Dept Quantum Sci, Acton, ACT 2000, Australia.
   [Gilles, F.; Herding, M.; Nicklaus, K.] SpaceTech GmbH Immenstaad, D-88090 Immenstaad, Germany.
   [Brown, J.; Dligatch, S.; Farrant, D. I.; Green, K. L.; Seckold, J. A.] CSIRO Mat Sci & Engn, Australian Ctr Precis Opt, Lindfield, NSW 2070, Australia.
   [Burke, J.] BIAS Bremer Inst Angew Strahltech gGmbH, Abt Opt Messtech, D-28359 Bremen, Germany.
   [Blundell, M.; Brister, R.; Smith, C.] Electro Opt Syst Pty Ltd, Mt Stromlo Observ, Weston, ACT 2611, Australia.
   [Sheard, B. S.; Heinzel, G.; Danzmann, K.] Leibniz Univ Hannover, Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
   [Sheard, B. S.; Heinzel, G.; Danzmann, K.] Leibniz Univ Hannover, Inst Gravitat Phys, D-30167 Hannover, Germany.
   [Klipstein, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Fleddermann, R (reprint author), Australian Natl Univ, Dept Quantum Sci, 2 Sci Rd, Acton, ACT 2000, Australia.
EM Roland.Fleddermann@anu.edu.au
RI McClelland, David/E-6765-2010; Farrant, David/A-4028-2008; Shaddock,
   Daniel/A-7534-2011; Ward, Robert/I-8032-2014
OI McClelland, David/0000-0001-6210-5842; Shaddock,
   Daniel/0000-0002-6885-3494; Ward, Robert/0000-0001-5503-5241
FU Australian Space Research Program; German Federal Ministry of Education
   and Research; German Aerospace Centre; Australia's Commonwealth
   Scientific and Industrial Research Organisation; Deutsche
   Forschungsgemeinschaft (DFG); Excellence QUEST
FX The TMA development was funded by the Australian Space Research Program,
   an initiative of the Australian Government, with contributions from the
   German Federal Ministry of Education and Research, the German Aerospace
   Centre, Australia's Commonwealth Scientific and Industrial Research
   Organisation, and the Deutsche Forschungsgemeinschaft (DFG) within the
   Cluster of Excellence QUEST (Centre for Quantum Engineering and
   Space-Time Research).
NR 12
TC 2
Z9 2
U1 3
U2 7
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 OCT 7
PY 2014
VL 31
IS 19
AR 195004
DI 10.1088/0264-9381/31/19/195004
PG 12
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
   & Fields
SC Astronomy & Astrophysics; Physics
GA AR2JU
UT WOS:000343411400004
ER

PT J
AU Boys, BL
   Martin, RV
   van Donkelaar, A
   MacDonell, RJ
   Hsu, NC
   Cooper, MJ
   Yantosca, RM
   Lu, Z
   Streets, DG
   Zhang, Q
   Wang, SW
AF Boys, B. L.
   Martin, R. V.
   van Donkelaar, A.
   MacDonell, R. J.
   Hsu, N. C.
   Cooper, M. J.
   Yantosca, R. M.
   Lu, Z.
   Streets, D. G.
   Zhang, Q.
   Wang, S. W.
TI Fifteen-Year Global Time Series of Satellite-Derived Fine Particulate
   Matter
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID LONG-TERM TREND; AEROSOL OPTICAL-THICKNESS; AIR-POLLUTION; RIVER DELTA;
   CHINA; CALIBRATION; VISIBILITY; PM2.5; MISR; PERSPECTIVE
AB Ambient fine particulate matter (PM2.5) is a leading environmental risk factor for premature mortality. We use aerosol optical depth (AOD) retrieved from two satellite instruments, MISR and SeaWiFS, to produce a unified 15-year global time series (1998-2012) of ground-level PM2.5 concentration at a resolution of 1 degrees x 1 degrees. The GEOS-Chem chemical transport model (CTM) is used to relate each individual AOD retrieval to ground-level PM2.5. Four broad areas showing significant, spatially coherent, annual trends are examined in detail: the Eastern U.S. (-0.39 +/- 0.10 mu g m(-3) yr(-1)), the Arabian Peninsula (0.81 +/- 0.21 mu g m(-3) yr(-1)), South Asia (0.93 +/- 0.22 mu g m(-3) yr(-1)) and East Asia (0.79 +/- 0.27 mu g m(-3) yr(-1)). Over the period of dense in situ observation (1999-2012), the linear tendency for the Eastern U.S. (-0.37 +/- 0.13 mu g m(-3) yr(-1)) agrees well with that from in situ measurements (-0.38 +/- 0.06 mu g m(-3) yr(-1)). A GEOS-Chem simulation reveals that secondary inorganic aerosols largely explain the observed PM2.5 trend over the Eastern U.S., South Asia, and East Asia, while mineral dust largely explains the observed trend over the Arabian Peninsula.
C1 [Boys, B. L.; Martin, R. V.; van Donkelaar, A.; MacDonell, R. J.; Cooper, M. J.] Dalhousie Univ, Halifax, NS, Canada.
   [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Hsu, N. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Yantosca, R. M.] Harvard Univ, Cambridge, MA 02138 USA.
   [Lu, Z.; Streets, D. G.] Argonne Natl Lab, Argonne, IL 60439 USA.
   [Zhang, Q.; Wang, S. W.] Tsinghua Univ, Ctr Earth Syst Sci, Beijing 100084, Peoples R China.
RP Boys, BL (reprint author), Dalhousie Univ, Halifax, NS, Canada.
EM briboys@gmail.com
RI Chem, GEOS/C-5595-2014; Zhang, Qiang/D-9034-2012; Martin,
   Randall/C-1205-2014
OI Martin, Randall/0000-0003-2632-8402
FU NSERC Canada; Izaak Walton Killiam Memorial Scholarship
FX Funding for this work was provided by NSERC Canada and by an Izaak
   Walton Killiam Memorial Scholarship for B. L. Boys. Computational
   facilities are partially provided by ACEnet, the regional high
   performance computing consortium for universities in Atlantic Canada. We
   thank the AERONET, MISR, SeaWiFS, CALIPSO, IMPROVE, and AQS science
   teams for making their data publicly available.
NR 65
TC 36
Z9 36
U1 9
U2 68
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
EI 1520-5851
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD OCT 7
PY 2014
VL 48
IS 19
BP 11109
EP 11118
DI 10.1021/es502113p
PG 10
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA AQ7RJ
UT WOS:000343016600014
PM 25184953
ER

PT J
AU Briggs, RM
   Frez, C
   Borgentun, CE
   Forouhar, S
AF Briggs, Ryan M.
   Frez, Clifford
   Borgentun, Carl E.
   Forouhar, Siamak
TI Regrowth-free single-mode quantum cascade lasers with power consumption
   below 1W
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID DIODE-LASERS; SPECTROSCOPY; DISSIPATION
AB We report on single-mode distributed-feedback quantum cascade lasers emitting at 4.8 mu m with continuous-wave threshold power consumption as low as 0.76 W at 20 degrees C and 0.98 W at 50 degrees C. Following growth of the laser active region and semiconductor cladding layers by a single molecular beam epitaxy process, devices with 4-mu m-wide ridges and vertical sidewall gratings were fabricated using plasma etching and standard dielectric and metal deposition processes. In terms of mode stability, output power, and efficiency, we show that lasers with 1-mm cavity length and high-reflectivity back-facet coatings can match the performance of buried heterostructure devices, but with the advantage of requiring only a single epitaxial growth step. (C) 2014 AIP Publishing LLC.
C1 [Briggs, Ryan M.; Frez, Clifford; Borgentun, Carl E.; Forouhar, Siamak] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Briggs, RM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ryan.m.briggs@jpl.nasa.gov
RI Chen, Ru/A-5105-2015
NR 23
TC 6
Z9 6
U1 1
U2 40
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
   MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD OCT 6
PY 2014
VL 105
IS 14
AR 141117
DI 10.1063/1.4898003
PG 4
WC Physics, Applied
SC Physics
GA AS5ZC
UT WOS:000344343900017
ER

PT J
AU Valivarthi, R
   Lucio-Martinez, I
   Rubenok, A
   Chan, P
   Marsili, F
   Verma, VB
   Shaw, MD
   Stern, JA
   Slater, JA
   Oblak, D
   Nam, SW
   Tittel, W
AF Valivarthi, R.
   Lucio-Martinez, I.
   Rubenok, A.
   Chan, P.
   Marsili, F.
   Verma, V. B.
   Shaw, M. D.
   Stern, J. A.
   Slater, J. A.
   Oblak, D.
   Nam, S. W.
   Tittel, W.
TI Efficient Bell state analyzer for time-bin qubits with fast-recovery WSi
   superconducting single photon detectors
SO OPTICS EXPRESS
LA English
DT Article
ID QUANTUM COMMUNICATION; TELEPORTATION; CRYPTOGRAPHY
AB We experimentally demonstrate a high-efficiency Bell state measurement for time-bin qubits that employs two superconducting nanowire single-photon detectors with short dead-times, allowing projections onto two Bell states, vertical bar psi(-)> and vertical bar psi(+)>. Compared to previous implementations for time-bin qubits, this yields an increase in the efficiency of Bell state analysis by a factor of thirty. (C) 2014 Optical Society of America
C1 [Valivarthi, R.; Lucio-Martinez, I.; Rubenok, A.; Chan, P.; Slater, J. A.; Oblak, D.; Tittel, W.] Univ Calgary, Inst Quantum Sci & Technol, Calgary, AB T2N 1N4, Canada.
   [Valivarthi, R.; Lucio-Martinez, I.; Rubenok, A.; Slater, J. A.; Oblak, D.; Tittel, W.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
   [Chan, P.] Univ Calgary, Dept Elect & Comp Engn, Calgary, AB T2N 1N4, Canada.
   [Verma, V. B.; Nam, S. W.] NIST, Boulder, CO 80305 USA.
   [Marsili, F.; Shaw, M. D.; Stern, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Valivarthi, R (reprint author), Univ Calgary, Inst Quantum Sci & Technol, Calgary, AB T2N 1N4, Canada.
EM vrrvaliv@ucalgary.ca
RI Slater, Joshua/F-2523-2011; Tittel, Wolfgang/A-1600-2011
FU Alberta Innovates Technology Futures (AITF); National Sciences and
   Engineering Research Council of Canada (NSERC); US Defense Advanced
   Research Projects Agency (DARPA) Quiness Program [W31P4Q-13-1-0004];
   Killam Trusts; DARPA Information in a Photon (InPho) program
FX WT, JAS, PC, AR, RV, ILM and DO thank Neil Sinclair and Vladimir
   Kiselyov for discussions and technical support, and acknowledge funding
   by Alberta Innovates Technology Futures (AITF), the National Sciences
   and Engineering Research Council of Canada (NSERC), the US Defense
   Advanced Research Projects Agency (DARPA) Quiness Program under Grant
   No. W31P4Q-13-1-0004, and the Killam Trusts. VBV and SWN acknowledge
   partial funding for detector development from the 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 25
TC 9
Z9 9
U1 1
U2 16
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 OCT 6
PY 2014
VL 22
IS 20
BP 24497
EP 24506
DI 10.1364/OE.22.024497
PG 10
WC Optics
SC Optics
GA AQ4IE
UT WOS:000342757000073
PM 25322025
ER

PT J
AU Chandrasekhar, P
   Zay, BJ
   Lawrence, D
   Caldwell, E
   Sheth, R
   Stephan, R
   Cornwell, J
AF Chandrasekhar, Prasanna
   Zay, Brian J.
   Lawrence, David
   Caldwell, Edmonia
   Sheth, Rubik
   Stephan, Ryan
   Cornwell, John
TI Variable-Emittance Infrared Electrochromic Skins Combining Unique
   Conducting Polymers, Ionic Liquid Electrolytes, Microporous Polymer
   Membranes, and Semiconductor/Polymer Coatings, for Spacecraft Thermal
   Control
SO JOURNAL OF APPLIED POLYMER SCIENCE
LA English
DT Article
DE applications; conducting polymers; electrochemistry; ionic liquids;
   optical and photovoltaic applications
ID ELECTROCHEMICAL DEVICES
AB Variable emittance (e) is a property vital for the increasing needs in thermal control of future microspacecraft. This article describes fabrication, function, and performance of thin-film, flexible, variable-emittance (V-E) electrochromic skins that use a conducting polymer/-Au/-microporous membrane (CP/Au/mP) base, and a new, unique ionic liquid electrolyte (IonEl). Poly(aniline-codiphenyl amine) with a long-chain polymeric dopant is used as the CP. A unique, patented device design yields no barrier between the active, electrochromic CP surface and the external environment, except for a thin, infrared-transparent semiconductor/polymer film that lowers solar absorptance [alpha(s)] and protects from atomic-O/far-UV. Use of the IonEl requires special activation methods. Data presented show tailorable e variations from 0.19 to 0.90, De values of >0.50 (which is the highest reported thus far for any functional V-E material, to our knowledge), alpha(s) < 0.35, and nearly indefinite cyclability. Extended space durability testing, including calorimetric thermal vacuum and continuous light/dark cycling over >7 months under space conditions (< 10(-5) Pa vacuum, far-UV), show excellent durability. Other data show resistance to solar wind, atomic-O, electrostatic discharge, and micrometeoroids. These lightweight, inexpensive, advanced polymeric materials represent the only technology that can work with micro- (<20 kg) and nano- (<2 kg) spacecraft, thus eventually allowing for much greater flexibility in their design and potentially "democratizing" the entire space industry, for example, allowing small firms to launch their own, dedicated satellites. (C) 2014 Wiley Periodicals, Inc.
C1 [Chandrasekhar, Prasanna; Zay, Brian J.; Lawrence, David] Ashwin Ushas Corp, Marlboro, NJ 07746 USA.
   [Caldwell, Edmonia] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Sheth, Rubik; Stephan, Ryan; Cornwell, John] NASA, Johnson Space Flight Ctr, Houston, TX 77058 USA.
RP Chandrasekhar, P (reprint author), Ashwin Ushas Corp, Marlboro, NJ 07746 USA.
EM chandra.p2@ashwin-ushas.com
FU National Aeronautics and Space Administration (NASA) (U.S.) [NNX12CA64C,
   NNX11CG21P, NNJ11HD02P, NNX09CA68C, NNX08CB96P]
FX Partial support of this work by the (U.S.) National Aeronautics and
   Space Administration (NASA) through Contract #s NNX12CA64C, NNX11CG21P,
   NNJ11HD02P, NNX09CA68C and NNX08CB96P to Ashwin-Ushas Corporation is
   gratefully acknowledged. The authors also thank the following for
   assistance: Dr. Gaj Birur, NASA-Jet Propulsion Laboratory, Pasadena, CA;
   Dr. Bruce Banks, NASA-Glenn Research Center, Dayton, OH; Mr. Dan
   Butler-NASA-Goddard Space Flight Center, Greenbelt, MD; Prof. J.R.
   Dennison, Materials Physics Group, Utah State University (USU-MPG), Salt
   Lake City, UT.
NR 79
TC 5
Z9 5
U1 8
U2 91
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0021-8995
EI 1097-4628
J9 J APPL POLYM SCI
JI J. Appl. Polym. Sci.
PD OCT 5
PY 2014
VL 131
IS 19
AR 40850
DI 10.1002/APP.40850
PG 15
WC Polymer Science
SC Polymer Science
GA AM9YV
UT WOS:000340238300037
ER

PT J
AU Shreiber, D
   Cravey, R
   Cole, MW
AF Shreiber, D.
   Cravey, R.
   Cole, M. W.
TI Numerical Simulations of a Metamaterial Based on an Array of Complex
   Oxide Thin Film Infinite Rods for THz Applications
SO FERROELECTRICS
LA English
DT Article
DE Complex oxide thin films; THz dielectric metamaterials
AB Tunability of ferroelectric complex oxides is achieved by applied bias voltage. Many applications require usage of relatively low voltage which is achievable by using a ferroelectric thin-film. Recently developed dielectric metamaterials were implemented in bulk and in thick films. Metamaterials are resonant structures. The frequency range of 0.1-1.5 THz is of special interest for such applications as non-destructive evaluation of materials and detection of chemical and biological hazards. This paper numerically investigates the possibility of a resonant effect in a thin-film ferroelectric metamaterial and the effects of increased dielectric constant and thickness on the thin-film's resonance frequency.
C1 [Shreiber, D.; Cole, M. W.] US Army Res Lab, Weap & Mat Res Directorate, Aberdeen Proving Ground, MD 21005 USA.
   [Cravey, R.] NASA, Electromagnet & Sensors Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Shreiber, D (reprint author), US Army Res Lab, Weap & Mat Res Directorate, Aberdeen Proving Ground, MD 21005 USA.
EM daniel.shreiber.ctr@mail.mil
NR 9
TC 0
Z9 0
U1 3
U2 12
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0015-0193
EI 1563-5112
J9 FERROELECTRICS
JI Ferroelectrics
PD OCT 3
PY 2014
VL 470
IS 1
SI SI
BP 28
EP 34
DI 10.1080/00150193.2014.922781
PG 7
WC Materials Science, Multidisciplinary; Physics, Condensed Matter
SC Materials Science; Physics
GA AR1BV
UT WOS:000343316400008
ER

PT J
AU Hamid, AM
   Bera, PP
   Lee, TJ
   Aziz, SG
   Alyoubi, AO
   El-Shall, MS
AF Hamid, Ahmed M.
   Bera, Partha P.
   Lee, Timothy J.
   Aziz, Saadullah G.
   Alyoubi, Abdulrahman O.
   El-Shall, M. Samy
TI Evidence for the Formation of Pyrimidine Cations from the Sequential
   Reactions of Hydrogen Cyanide with the Acetylene Radical Cation
SO JOURNAL OF PHYSICAL CHEMISTRY LETTERS
LA English
DT Article
ID POLYCYCLIC AROMATIC-HYDROCARBON; INTERSTELLAR ICE ANALOGS; PREBIOTIC
   CHEMISTRY; ION CHEMISTRY; AMINO-ACIDS; GAS-PHASE; MOLECULES; DENSITY;
   MECHANISMS; METEORITES
AB Herein, we report the first direct evidence for the formation of pyrimidine ion isomers by sequential reactions of HCN with the acetylene radical cation in the gas phase at ambient temperature using the mass-selected variable temperature and pressure ion mobility technique. The formation and structures of the pyrimidine ion isomers are theoretically predicted via coupled cluster and density functional theory calculations. This ion molecule synthesis may indicate that pyrimidine is produced in the gas phase in space environments before being incorporated into condensed-phase ices and transformed into nucleic acid bases such as uracil.
C1 [Hamid, Ahmed M.; El-Shall, M. Samy] Virginia Commonwealth Univ, Dept Chem, Richmond, VA 23284 USA.
   [Bera, Partha P.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Bera, Partha P.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
   [Aziz, Saadullah G.; Alyoubi, Abdulrahman O.] King Abdulaziz Univ, Dept Chem, Jeddah 21589, Saudi Arabia.
RP El-Shall, MS (reprint author), Virginia Commonwealth Univ, Dept Chem, Box 2006, Richmond, VA 23284 USA.
EM Partha.P.Bera@nasa.gov; Timothy.J.Lee@nasa.gov; mselshal@vcu.edu
RI Lee, Timothy/K-2838-2012; Bera, Partha /K-8677-2012; Aziz,
   Saadullah/E-9648-2010; El-Shall, M. Samy/K-8954-2012
OI Aziz, Saadullah/0000-0003-1319-8784; El-Shall, M.
   Samy/0000-0002-1013-4948
FU National Science Foundation [CHE-0911146]; NASA Laboratory Astrophysics
   Carbon in the Galaxy consortium grant [NNH1OZDA001N]
FX This work was supported by the National Science Foundation
   (CHE-0911146). P.P.B. and T.J.L. gratefully acknowledge the support from
   the NASA Laboratory Astrophysics Carbon in the Galaxy consortium grant
   (NNH1OZDA001N).
NR 46
TC 7
Z9 7
U1 1
U2 24
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1948-7185
J9 J PHYS CHEM LETT
JI J. Phys. Chem. Lett.
PD OCT 2
PY 2014
VL 5
IS 19
BP 3392
EP 3398
DI 10.1021/jz501648q
PG 7
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
   Multidisciplinary; Physics, Atomic, Molecular & Chemical
SC Chemistry; Science & Technology - Other Topics; Materials Science;
   Physics
GA AQ8ID
UT WOS:000343067800008
PM 26278451
ER

PT J
AU Andrews-Hanna, JC
   Besserer, J
   Head, JW
   Howett, CJA
   Kiefer, WS
   Lucey, PJ
   McGovern, PJ
   Melosh, HJ
   Neumann, GA
   Phillips, RJ
   Schenk, PM
   Smith, DE
   Solomon, SC
   Zuber, MT
AF Andrews-Hanna, Jeffrey C.
   Besserer, Jonathan
   Head, James W., III
   Howett, Carly J. A.
   Kiefer, Walter S.
   Lucey, Paul J.
   McGovern, Patrick J.
   Melosh, H. Jay
   Neumann, Gregory A.
   Phillips, Roger J.
   Schenk, Paul M.
   Smith, David E.
   Solomon, Sean C.
   Zuber, Maria T.
TI Structure and evolution of the lunar Procellarum region as revealed by
   GRAIL gravity data
SO NATURE
LA English
DT Article
ID SOUTH-POLE; MARE VOLCANISM; KREEP TERRANE; ENCELADUS; ORIGIN; MOON;
   TOPOGRAPHY; INTERIOR; MERCURY; BASALTS
AB The Procellarum region is a broad area on the nearside of the Moon that is characterized by low elevations(1), thin crust(2), and high surface concentrations of the heat-producing elements uranium, thorium, and potassium(3,4). The region has been interpreted as an ancient impact basin approximately 3,200 kilometres in diameter(5-7), although supporting evidence at the surface would have been largely obscured as a result of the great antiquity and poor preservation of any diagnostic features. Here we use data from the Gravity Recovery and Interior Laboratory (GRAIL) mission(8) to examine the subsurface structure of Procellarum. The Bouguer gravity anomalies and gravity gradients reveal a pattern of narrow linear anomalies that border Procellarum and are interpreted to be the frozen remnants of lava-filled rifts and the underlying feeder dykes that served as the magma plumbing system for much of the nearside mare volcanism. The discontinuous surface structures that were earlier interpreted as remnants of an impact basin rim are shown in GRAIL data to be a part of this continuous set of border structures in a quasi-rectangular pattern with angular intersections, contrary to the expected circular or elliptical shape of an impact basin(9). The spatial pattern of magmatic-tectonic structures bounding Procellarum is consistent with their formation in response to thermal stresses produced by the differential cooling of the province relative to its surroundings, coupled with magmatic activity driven by the greater-than-average heat flux in the region.
C1 [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.
   [Besserer, Jonathan] 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.
   [Howett, Carly J. A.; Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA.
   [Kiefer, Walter S.; McGovern, Patrick J.; Schenk, Paul M.] Lunar & Planetary Inst, Houston, TX 77058 USA.
   [Lucey, Paul J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
   [Melosh, H. Jay] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA.
   [Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
   [Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
   [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
   [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
RP Andrews-Hanna, JC (reprint author), Colorado Sch Mines, Dept Geophys, Golden, CO 80401 USA.
EM jcahanna@mines.edu
RI Neumann, Gregory/I-5591-2013; 
OI Neumann, Gregory/0000-0003-0644-9944; McGovern,
   Patrick/0000-0001-9647-3096; Kiefer, Walter/0000-0001-6741-5460
FU NASA's GRAIL Guest Scientist Program [NNX12AL20G]
FX The GRAIL mission is a component of the NASA Discovery Program and is
   performed under contract to the Massachusetts Institute of Technology
   and the Jet Propulsion Laboratory, California Institute of Technology.
   J.C.A.-H. was supported by grant NNX12AL20G from NASA's GRAIL Guest
   Scientist Program.
NR 72
TC 16
Z9 16
U1 3
U2 29
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 OCT 2
PY 2014
VL 514
IS 7520
BP 68
EP +
DI 10.1038/nature13697
PG 19
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AP9SS
UT WOS:000342420800036
PM 25279919
ER

PT J
AU Andrews, LC
   Catania, GA
   Hoffman, MJ
   Gulley, JD
   Luthi, MP
   Ryser, C
   Hawley, RL
   Neumann, TA
AF Andrews, Lauren C.
   Catania, Ginny A.
   Hoffman, Matthew J.
   Gulley, Jason D.
   Luethi, Martin P.
   Ryser, Claudia
   Hawley, Robert L.
   Neumann, Thomas A.
TI Direct observations of evolving subglacial drainage beneath the
   Greenland Ice Sheet
SO NATURE
LA English
DT Article
ID HAUT GLACIER DAROLLA; WATER-PRESSURE; WEST GREENLAND; ABLATION ZONE;
   BASAL MOTION; SWITZERLAND; SURFACE; SYSTEM; FLOW; MELT
AB Seasonal acceleration of the Greenland Ice Sheet is influenced by the dynamic response of the subglacial hydrologic system to variability in meltwater delivery to the bed(1,2) via crevasses and moulins (vertical conduits connecting supraglacial water to the bed of the ice sheet). As the melt season progresses, the subglacial hydrologic system drains supraglacial meltwater more efficiently(1-4), decreasing basal water pressure(4) and moderating the ice velocity response to surface melting(1,2). However, limited direct observations of subglacial water pressure(4-7) mean that the spatiotemporal evolution of the subglacial hydrologic system remains poorly understood. Here we show that ice velocity is well correlated with moulin hydraulic head but is out of phase with that of nearby (0.3-2 kilometres away) boreholes, indicating that moulins connect to an efficient, channelized component of the subglacial hydrologic system, which exerts the primary control on diurnal and multi-day changes in ice velocity. Our simultaneous measurements of moulin and borehole hydraulic head and ice velocity in the Paakitsoq region of western Greenland show that decreasing trends in ice velocity during the latter part of the melt season cannot be explained by changes in the ability of moulin-connected channels to convey supraglacial melt. Instead, these observations suggest that decreasing late-season ice velocity may be caused by changes in connectivity in unchannelized regions of the subglacial hydrologic system. Understanding this spatiotemporal variability in subglacial pressures is increasingly important because melt-season dynamics affect ice velocity beyond the conclusion of the melt season(8-10).
C1 [Andrews, Lauren C.; Catania, Ginny A.; Gulley, Jason D.] Univ Texas Austin, Inst Geophys, Jackson Sch Geosci, Austin, TX 78758 USA.
   [Andrews, Lauren C.; Catania, Ginny A.; Ryser, Claudia] Univ Texas Austin, Dept Geol Sci, Jackson Sch Geosci, Austin, TX 78758 USA.
   [Hoffman, Matthew J.] Los Alamos Natl Lab, Fluid Dynam & Solid Mech Grp, Los Alamos, NM 87545 USA.
   [Hoffman, Matthew J.; Neumann, Thomas A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Gulley, Jason D.] Michigan Technol Univ, Dept Geol & Mining Engn & Sci, Houghton, MI 49931 USA.
   [Luethi, Martin P.] Univ Zurich, Dept Geog, Glaciol & Geomorphodynam Grp, Phys Geog Div, CH-8057 Zurich, Switzerland.
   [Luethi, Martin P.; Ryser, Claudia] Swiss Fed Inst Technol, Lab Hydraul Hydrol & Glaciol, CH-8093 Zurich, Switzerland.
   [Hawley, Robert L.] Dartmouth Coll, Dept Earth Sci, Hanover, NH 03755 USA.
RP Andrews, LC (reprint author), Univ Texas Austin, Inst Geophys, Jackson Sch Geosci, Austin, TX 78758 USA.
EM landrews@ig.utexas.edu
RI Catania, Ginny/B-9787-2008; Neumann, Thomas/D-5264-2012; Andrews,
   Lauren/D-8274-2017
OI Andrews, Lauren/0000-0003-3727-4737
FU United States National Science Foundation [OPP-0908156, OPP-0909454,
   ANT-0424589]; Swiss National Science Foundation [200021_127197];
   National Geographic Society [9067-12]; UTIG; NASA Cryospheric Sciences
   and Climate Modeling Programs within US Department of Energy, Office of
   Science; NSF [EAR-0946767]; NSF; NASA [EAR-0735156]; NSF OPP
   [ANT-1043681]
FX This project was supported by United States National Science Foundation
   grants OPP-0908156, OPP-0909454 and ANT-0424589 (to CReSIS), Swiss
   National Science Foundation grant 200021_127197, and National Geographic
   Society grant 9067-12. L. C. A. was also supported by UTIG Ewing-Worzel
   and Gale White Graduate Student Fellowships. M.J.H. was also supported
   by NASA Cryospheric Sciences and Climate Modeling Programs within the US
   Department of Energy, Office of Science. J.D.G. was also supported by an
   NSF Postdoctoral Fellowship (EAR-0946767). Logistical support was
   provided by CH2MHill Polar Services. The GPS base station and several
   on-ice GPS units were provided by the UNAVCO facility with support from
   the NSF and NASA under cooperative agreement EAR-0735156. The University
   of Minnesota Polar Geospatial Center, funded under NSF OPP collaborative
   agreement ANT-1043681, provided WorldView imagery. We thank K. M.
   Schild, J. A. MacGregor, J. D. Nowinski, B. F. Morriss and others for
   assistance in the field.
NR 47
TC 48
Z9 48
U1 7
U2 43
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 OCT 2
PY 2014
VL 514
IS 7520
BP 80
EP +
DI 10.1038/nature13796
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AP9SS
UT WOS:000342420800039
PM 25279921
ER

PT J
AU Connors, MM
   Mauro, R
   Statler, IC
AF Connors, Mary M.
   Mauro, Robert
   Statler, Irving C.
TI A Survey Methodology for Measuring Safety-Related Trends in the National
   Airspace System
SO INTERNATIONAL JOURNAL OF AVIATION PSYCHOLOGY
LA English
DT Article
ID MEMORY; MODEL
AB Making informed judgments about the effects of technological, human, or environmental changes on civil aviation requires reliable information. The National Aviation Operational Monitoring Service (NAOMS), a research project under NASA's Aviation Safety Program, developed and tested a survey methodology designed to provide statistically reliable information on changes over time in safety-related events in the national airspace. Such information would aid decision makers in determining what areas required attention. To evaluate the NAOMS concept, data from nearly 20,000 randomly selected air-carrier pilots were collected over 3 years. Results demonstrate that the NAOMS approach can reliably identify changes over time in the rates of safety-related events.
C1 [Connors, Mary M.; Statler, Irving C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Mauro, Robert] Decis Res, Eugene, OR USA.
   [Mauro, Robert] Univ Oregon, Dept Psychol, Eugene, OR 97403 USA.
RP Connors, MM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM mary.connors@nasa.gov
NR 22
TC 0
Z9 0
U1 0
U2 2
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 1050-8414
EI 1532-7108
J9 INT J AVIAT PSYCHOL
JI Int. J. Aviat. Psychol.
PD OCT 2
PY 2014
VL 24
IS 4
BP 265
EP 286
DI 10.1080/10508414.2014.949202
PG 22
WC Psychology, Applied
SC Psychology
GA AQ0WT
UT WOS:000342504100002
ER

PT J
AU Verma, S
   Kozon, T
   Ballinger, D
AF Verma, Savita
   Kozon, Thomas
   Ballinger, Debbi
TI Comparative Analysis of Procedures for Dual and Triple Closely Spaced
   Parallel Runways
SO INTERNATIONAL JOURNAL OF AVIATION PSYCHOLOGY
LA English
DT Article
AB This article provides a comparative analysis of 2 experiments on procedures to increase the capacity of closely spaced parallel runways under low-visibility conditions. The common goal for both studies was to achieve visual meteorological capacity under instrument meteorological conditions, when landing aircraft on parallel runways 750 ft apart. Using a high-fidelity flight deck simulator, both studies investigated procedures related to breakout maneuvers on final approach during off-nominal conditions. The first study investigated procedures for 2 parallel runways (involving a leading and trailing aircraft) and the second study examined 3 parallel runways separated by 750 ft, investigating procedures for 3 simultaneously arriving aircraft (leading, center, and right aircraft). In both studies, off-nominal events were introduced during the approach. In some cases the wake of the leading aircraft drifted too close to the aircraft behind. In others, the leading aircraft deviated off its course and blundered toward the trailing aircraft. Statistical analysis examined the effects of approach echelon (2-runway vs. 3-runway), breakout cause, and breakout location on the dependent measures of breakout trajectory cross-track error, breakout trajectory track angle error, pilot workload, and pilot situation awareness. Although revealing differences between the study conditions, results also show accurate cross-track and track angle error levels (i.e., high levels of breakout trajectory accuracy), manageable pilot workload, and high levels of pilot situation awareness across all conditions in both studies. Results suggest possible avenues of future adaptation of dual and triple parallel runway operations (e.g., improving pilot training) and also show potential promise of the concept.
C1 [Verma, Savita; Kozon, Thomas; Ballinger, Debbi] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Kozon, Thomas] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
RP Verma, S (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM savita.a.verma@nasa.gov
NR 14
TC 0
Z9 0
U1 2
U2 4
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 CHESTNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 1050-8414
EI 1532-7108
J9 INT J AVIAT PSYCHOL
JI Int. J. Aviat. Psychol.
PD OCT 2
PY 2014
VL 24
IS 4
BP 315
EP 336
DI 10.1080/10508414.2014.949519
PG 22
WC Psychology, Applied
SC Psychology
GA AQ0WT
UT WOS:000342504100005
ER

PT J
AU Hutyra, LR
   Duren, R
   Gurney, KR
   Grimm, N
   Kort, EA
   Larson, E
   Shrestha, G
AF Hutyra, Lucy R.
   Duren, Riley
   Gurney, Kevin R.
   Grimm, Nancy
   Kort, Eric A.
   Larson, Elisabeth
   Shrestha, Gyami
TI Urbanization and the carbon cycle: Current capabilities and research
   outlook from the natural sciences perspective
SO EARTHS FUTURE
LA English
DT Review
ID GREENHOUSE-GAS EMISSIONS; ATMOSPHERIC CO2 INVERSIONS; UNITED-STATES;
   CLIMATE-CHANGE; METROPOLITAN-AREA; DIOXIDE EMISSIONS; URBAN
   ENVIRONMENTS; HUMAN-SETTLEMENTS; PIPELINE LEAKS; METHANE LEAKS
AB This paper explores the urban carbon cycle from the natural sciences perspective, identifying key knowledge gaps and priority areas for future research. The combination of large, concentrated carbon fluxes and rapid change makes cities key elements of the carbon cycle and offers the potential for them to serve as "first responders" for climate action. Estimates of urban-scale carbon fluxes are significantly more uncertain than at larger spatial scales, in part because past studies have mostly avoided local/urban scales where the mix of anthropogenic and natural fluxes is complex and difficult to observationally isolate. To develop effective emission reduction policies, we need to understand emission sources and how they may be changing. Such improved quantification and understanding of underlying processes at the urban scale will not only provide policy-relevant information and improve the understanding of urban dynamics and future scenarios, but will also translate into better global-scale anthropogenic flux estimates, and advance our understanding of carbon cycle and climate feedbacks across multiple scales. Understanding the relationship between urbanization and urban carbon flows requires intellectual integration with research communities beyond the natural sciences. Cities can serve as interdisciplinary process laboratories that are sufficiently constrained in both spatial and governance scale to support truly integrated research by the natural sciences, social sciences, and engineering. A thoughtfully crafted science research agenda that is grounded in sustained, dense observations relevant to estimating urban carbon fluxes and their controlling processes and is focused on a statistically significant sample of cities will advance our understanding of the carbon cycle.
C1 [Hutyra, Lucy R.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
   [Duren, Riley] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA.
   [Gurney, Kevin R.; Grimm, Nancy] Arizona State Univ, Sch Life Sci, Sch Sustainabil, Tempe, AZ USA.
   [Kort, Eric A.] Univ Michigan, Coll Engn, Ann Arbor, MI 48109 USA.
   [Larson, Elisabeth] NASA, Div Earth Sci, Washington, DC 20546 USA.
   [Shrestha, Gyami] US Global Change Res Program UCAR, US Carbon Cycle Sci Program, Washington, DC USA.
RP Hutyra, LR (reprint author), Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
EM lrhutyra@bu.edu
RI Kort, Eric/F-9942-2012; Grimm, Nancy/D-2840-2009; Shrestha,
   Gyami/F-9118-2014
OI Kort, Eric/0000-0003-4940-7541; Grimm, Nancy/0000-0001-9374-660X;
   Shrestha, Gyami/0000-0001-7150-8731
FU NSF [DEB-1149471, 0846358, BTS1026865]; NASA [NNX12AM82G]; National
   Institute for Standards and Technology [104336]; Carbon Cycle
   Interagency Working Group (CCIWG)
FX LR Hutyra is supported in this research by NSF CAREER award DEB-1149471
   and NASA Interdisciplinary Science award NNX12AM82G. R Duren's research
   was done at the Jet Propulsion Laboratory, a division of the California
   Institute of Technology under contract to the National Aeronautics and
   Space Administration. KR Gurney is supported in this research by NSF
   CAREER award 0846358 and National Institute for Standards and Technology
   grant 104336. N Grimm was supported by NSF BTS1026865. The October
   14-17, 2013 Workshop on Human-Carbon Interactions in Urban Systems
   sponsored by the Carbon Cycle Interagency Working Group (CCIWG) and US
   Carbon Cycle Program provided the platform for this research. The data
   presented in this review paper are synthesized from existing literature;
   the corresponding author can be contacted directly for additional
   information.
NR 168
TC 19
Z9 19
U1 18
U2 58
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2328-4277
J9 EARTHS FUTURE
JI Earth Future
PD OCT
PY 2014
VL 2
IS 10
BP 473
EP 495
DI 10.1002/2014EF000255
PG 23
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
   Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
   Sciences
GA CN0WY
UT WOS:000358136100002
ER

PT J
AU Romero-Lankao, P
   Gurney, KR
   Seto, KC
   Chester, M
   Duren, RM
   Hughes, S
   Hutyra, LR
   Marcotullio, P
   Baker, L
   Grimm, NB
   Kennedy, C
   Larson, E
   Pincetl, S
   Runfola, D
   Sanchez, L
   Shrestha, G
   Feddema, J
   Sarzynski, A
   Sperling, J
   Stokes, E
AF Romero-Lankao, Patricia
   Gurney, Kevin R.
   Seto, Karen C.
   Chester, Mikhail
   Duren, Riley M.
   Hughes, Sara
   Hutyra, Lucy R.
   Marcotullio, Peter
   Baker, Lawrence
   Grimm, Nancy B.
   Kennedy, Christopher
   Larson, Elisabeth
   Pincetl, Stephanie
   Runfola, Dan
   Sanchez, Landy
   Shrestha, Gyami
   Feddema, Johannes
   Sarzynski, Andrea
   Sperling, Joshua
   Stokes, Eleanor
TI A critical knowledge pathway to low-carbon, sustainable futures:
   Integrated understanding of urbanization, urban areas, and carbon
SO EARTHS FUTURE
LA English
DT Article
ID GLOBAL ENVIRONMENTAL-CHANGE; UNITED-STATES; TECHNOLOGICAL TRANSITIONS;
   POLITICAL ECOLOGY; CITIES; EMISSIONS; SYSTEMS; INDIA; FRAMEWORK; CITY
AB Independent lines of research on urbanization, urban areas, and carbon have advanced our understanding of some of the processes through which energy and land uses affect carbon. This synthesis integrates some of these diverse viewpoints as a first step toward a coproduced, integrated framework for understanding urbanization, urban areas, and their relationships to carbon. It suggests the need for approaches that complement and combine the plethora of existing insights into interdisciplinary explorations of how different urbanization processes, and socio-ecological and technological components of urban areas, affect the spatial and temporal patterns of carbon emissions, differentially over time and within and across cities. It also calls for a more holistic approach to examining the carbon implications of urbanization and urban areas, based not only on demographics or income but also on other interconnected features of urban development pathways such as urban form, economic function, economic-growth policies, and other governance arrangements. It points to a wide array of uncertainties around the urbanization processes, their interactions with urban socio-institutional and built environment systems, and how these impact the exchange of carbon flows within and outside urban areas. We must also understand in turn how carbon feedbacks, including carbon impacts and potential impacts of climate change, can affect urbanization processes. Finally, the paper explores options, barriers, and limits to transitioning cities to low-carbon trajectories, and suggests the development of an end-to-end, coproduced and integrated scientific understanding that can more effectively inform the navigation of transitional journeys and the avoidance of obstacles along the way.
C1 [Romero-Lankao, Patricia; Sperling, Joshua] Natl Ctr Atmospher Res, Urban Futures, Boulder, CO 80307 USA.
   [Gurney, Kevin R.; Grimm, Nancy B.] Arizona State Univ, Sch Life Sci, Global Inst Sustainabil, Tempe, AZ USA.
   [Seto, Karen C.; Stokes, Eleanor] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA.
   [Chester, Mikhail] Arizona State Univ, Sch Civil Environm & Sustainable Engn, Phoenix, AZ USA.
   [Duren, Riley M.] NASA, Jet Prop Lab, Pasadena, CA USA.
   [Hughes, Sara] Univ Toronto Mississauga, Dept Polit Sci, Toronto, ON, Canada.
   [Hutyra, Lucy R.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA.
   [Marcotullio, Peter] CUNY Hunter Coll, Dept Geog, New York, NY 10021 USA.
   [Baker, Lawrence] Univ Minnesota, Dept Bioprod & Biosyst Engn, St Paul, MN 55108 USA.
   [Kennedy, Christopher] Univ Toronto, Dept Civil Engn, Toronto, ON, Canada.
   [Larson, Elisabeth] NASA, Terr Ecol Program, Div Earth Sci, Washington, DC 20546 USA.
   [Pincetl, Stephanie] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA USA.
   [Runfola, Dan] Coll William & Mary, Inst Theory & Practice Int Relat, AidData, Williamsburg, VA USA.
   [Sanchez, Landy] El Colegio Mexico, Ctr Estudios Demog Urbanos & Ambientales, Mexico City, DF, Mexico.
   [Shrestha, Gyami] UCAR, US Carbon Cycle Sci Program, US Global Change Res Program, Washington, DC USA.
   [Feddema, Johannes] Univ Kansas, Dept Geog, Lawrence, KS 66045 USA.
   [Sarzynski, Andrea] Univ Delaware, George Sch Publ Policy & Adm, Newark, DE USA.
RP Romero-Lankao, P (reprint author), Natl Ctr Atmospher Res, Urban Futures, POB 3000, Boulder, CO 80307 USA.
EM prlankao@ucar.edu
RI Grimm, Nancy/D-2840-2009; Shrestha, Gyami/F-9118-2014; 
OI Grimm, Nancy/0000-0001-9374-660X; Shrestha, Gyami/0000-0001-7150-8731;
   Sarzynski, Andrea/0000-0001-9941-5764; Stokes, Eleanor
   C./0000-0002-0204-8847
NR 82
TC 9
Z9 9
U1 7
U2 33
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2328-4277
J9 EARTHS FUTURE
JI Earth Future
PD OCT
PY 2014
VL 2
IS 10
BP 515
EP 532
DI 10.1002/2014EF000258
PG 18
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
   Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
   Sciences
GA CN0WY
UT WOS:000358136100004
ER

PT J
AU Ivler, CM
   Powell, JD
   Tischler, MB
   Fletcher, JW
   Ott, C
AF Ivler, Christina M.
   Powell, J. David
   Tischler, Mark B.
   Fletcher, Jay W.
   Ott, Carl
TI Design and Flight Test of a Cable Angle Feedback Flight Control System
   for the RASCAL JUH-60 Helicopter
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
AB The ability of a helicopter to carry externally slung loads makes it very versatile for many civil and military operations. However, the piloted handling qualities of the helicopter are degraded by the presence of the slung load. A control system is developed that uses measurements of the slung load motions as well as conventional fuselage feedback to improve the handling qualities for hover/low-speed operations. Prior research has shown a fundamental trade-off between load damping and piloted handling qualities for a feedback control system with cable angle/rate feedback. A new task-tailored approach proposed and implemented herein uses a method of switching between a load damping mode and a piloted handling qualities mode. These modes provide appropriate load feedback depending on the piloting task and flight regime. This provides improved handling qualities for maneuvering flight and for improved precision load control at hover. A new mission task element for precision load placement is developed (for possible inclusion into ADS-33E-PRF) to test the ability of the cable feedback system to improve load placement task performance. The improvements provided by this control system are demonstrated in a piloted flight test on the JUH-60A RASCAL fly-by-wire helicopter. The average load set-down time was reduced by a factor of two for the 1000-lb load on a 56-ft sling.
C1 [Ivler, Christina M.] US Army RDECOM, Aviat Dev Directorate AFDD AMRDEC, Moffett Field, CA 94035 USA.
   [Powell, J. David] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
   [Tischler, Mark B.; Fletcher, Jay W.; Ott, Carl] US Army RDECOM, Aviat Dev Directorate AFDD AMRDEC, Ames Res Ctr, Moffett Field, CA USA.
RP Ivler, CM (reprint author), US Army RDECOM, Aviat Dev Directorate AFDD AMRDEC, Moffett Field, CA 94035 USA.
EM christina.ivler@us.army.mil
NR 23
TC 2
Z9 2
U1 0
U2 0
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
EI 2161-6027
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD OCT
PY 2014
VL 59
IS 4
AR 042008
DI 10.4050/JAHS.59.042008
PG 15
WC Engineering, Aerospace
SC Engineering
GA AZ7YT
UT WOS:000348432300009
ER

PT J
AU Mettler, B
   Kong, ZD
   Goerzen, C
   Whalley, M
AF Mettler, Berenice
   Kong, Zhaodan
   Goerzen, Chad
   Whalley, Matthew
TI Guidance Performance Benchmarking for Autonomous Rotorcraft
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
AB This paper describes a framework for performance evaluation of autonomous guidance systems. The elements of the framework consist of a set of spatial geometries, flight tasks, performance metrics, a flightdynamic model, and baseline solutions. The spatial benchmarks consist of six tasks in simple geometrical environments and 10 tasks inmore complex urban environments based on a real digital terrain elevation map. The framework also includes a set of performance metrics used to compare trajectories. The performance baselines used in the proposed framework are near-optimal solutions computed using one of two trajectory optimization methods: numerical optimization based on nonlinear programming for the simple geometric environments and a motion primitive automaton for problems involving the urban environments. The paper concludes with a demonstration of the benchmarking framework using the Obstacle Field Navigation system developed by the Army Aeroflightdynamics Directorate.
C1 [Mettler, Berenice; Kong, Zhaodan] Univ Minnesota, Dept Aerosp Engn & Mech, Interact Guidance & Control Lab, Minneapolis, MN 55455 USA.
   [Goerzen, Chad] San Jose State Univ, Res Fdn, Ames Res Ctr, Moffett Field, CA USA.
   [Whalley, Matthew] US Army Res, Aeroflightdynam Directorate AMRDEC, Dev Engn Command Ames Res Ctr, Moffett Field, CA USA.
RP Mettler, B (reprint author), Univ Minnesota, Dept Aerosp Engn & Mech, Interact Guidance & Control Lab, Minneapolis, MN 55455 USA.
EM mettler@umn.edu
RI Kong, Zhaodan/E-9362-2015
OI Kong, Zhaodan/0000-0002-2493-1366
FU NASA Ames [NNX07AN31A]
FX This research work was enabled thanks to the financial support of NASA
   Ames (grant number NNX07AN31A).
NR 25
TC 0
Z9 0
U1 0
U2 2
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
EI 2161-6027
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD OCT
PY 2014
VL 59
IS 4
AR 042009
DI 10.4050/JAHS.59.042009
PG 16
WC Engineering, Aerospace
SC Engineering
GA AZ7YT
UT WOS:000348432300010
ER

PT J
AU Raz, R
   Rosen, A
   Cicolani, LS
   Lusardi, J
AF Raz, Reuben
   Rosen, Aviv
   Cicolani, Luigi S.
   Lusardi, Jeffery
TI Using Wind Tunnel Tests for Slung-Load Clearance, Part 1: The CONEX
   Cargo Container
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
AB Previously, the authors showed that dynamic wind tunnel tests of a suspended CONEX cargo container model exhibited encouraging levels of success in predicting the stability characteristics and speed envelope of the full-scale load. The present study includes further use of the UH-60/CONEX system to investigate effects that were observed previously, but not fully addressed. These effects include the influence of pilot inputs and helicopter motions on the coupled pilot/helicopter/slung-load dynamics, the influence of center of gravity offset of the slung load, and the behavior of a load when a yaw swivel is not used in the suspension. It is shown that all three effects are important and affect the slung-load dynamics. The capability of wind tunnel tests to predict the behavior of slung loads in flight is shown for these effects.
C1 [Raz, Reuben; Rosen, Aviv] Technion Israel Inst Technol, Fac Aerosp Engn, IL-32000 Haifa, Israel.
   [Cicolani, Luigi S.] San Jose State Univ, Res Fdn, San Jose, CA 95192 USA.
   [Cicolani, Luigi S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Lusardi, Jeffery] US Army, Aviat Dev Directorate, AFDD Aviat & Missile Res, Dev & Engn Ctr Res,Ames Res Ctr, Moffett Field, CA USA.
RP Rosen, A (reprint author), Technion Israel Inst Technol, Fac Aerosp Engn, IL-32000 Haifa, Israel.
EM rosen@aerodyne.technion.ac.il
NR 18
TC 3
Z9 3
U1 1
U2 1
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
EI 2161-6027
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD OCT
PY 2014
VL 59
IS 4
AR 042003
DI 10.4050/JAHS.59.042003
PG 12
WC Engineering, Aerospace
SC Engineering
GA AZ7YT
UT WOS:000348432300004
ER

PT J
AU Raz, R
   Rosen, A
   Cicolani, LS
   Lusardi, J
   Gassaway, B
   Thompson, T
AF Raz, Reuben
   Rosen, Aviv
   Cicolani, Luigi S.
   Lusardi, Jeffery
   Gassaway, Bryan
   Thompson, Tom
TI Using Wind Tunnel Tests for Slung-Load Clearance, Part 2: Other Loads
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
AB The first new load is the TRIO container that can be flown in three configurations with different heights. The second new load is a ribbon bridge interior bay section. Wind tunnel results with models of the new loads exhibit in general good agreement with flight-test results. The results of the new loads strengthen further the approach of using wind tunnel tests to accelerate slung-load clearance, as well as reduce risk and cost.
C1 [Raz, Reuben; Rosen, Aviv] Technion Israel Inst Technol, Fac Aerosp Engn, IL-32000 Haifa, Israel.
   [Cicolani, Luigi S.] San Jose State Univ, Res Fdn, San Jose, CA 95192 USA.
   [Lusardi, Jeffery] US Army, Aviat Dev Directorate, AFDD Aviat & Missile Res, Dev & Engn Ctr Res,Ames Res Ctr, Moffett Field, CA USA.
   [Gassaway, Bryan; Thompson, Tom] US Army, Aviat Engn Directorate, Aeromech Div, Redstone Arsenal, AL USA.
RP Rosen, A (reprint author), Technion Israel Inst Technol, Fac Aerosp Engn, IL-32000 Haifa, Israel.
EM rosen@aerodyne.technion.ac.il
NR 10
TC 2
Z9 2
U1 1
U2 2
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
EI 2161-6027
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD OCT
PY 2014
VL 59
IS 4
AR 042004
DI 10.4050/JAHS.59.042004
PG 12
WC Engineering, Aerospace
SC Engineering
GA AZ7YT
UT WOS:000348432300005
ER

PT J
AU Weng, QH
   Hu, XF
   Quattrochi, DA
   Liu, H
AF Weng, Qihao
   Hu, Xuefei
   Quattrochi, Dale A.
   Liu, Hua
TI Assessing Intra-Urban Surface Energy Fluxes Using Remotely Sensed ASTER
   Imagery and Routine Meteorological Data: A Case Study in Indianapolis,
   USA
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
   SENSING
LA English
DT Article
DE Intra-urban variability; seasonality; surface energy fluxes; urban heat
   island; urban remote sensing
ID SENSIBLE HEAT-FLUX; URBAN AREAS; IMPERVIOUS SURFACES; BALANCE ALGORITHM;
   NET-RADIATION; TEMPERATURES; EMISSIVITY; ROUGHNESS; CANOPY; ISLAND
AB The seasonal and spatial variability of surface heat fluxes is crucial to the understanding of urban heat island phenomenon and dynamics. To estimate energy fluxes, remote sensing derived biophysical variables need to be integrated with surface atmospheric parameters measured in meteorological stations or in situ field measurements. In this study, based on the two-source energy balance algorithm, we applied a method to estimate surface energy fluxes by combined use of multispectral ASTER images and routine meteorological data, and applied it to the City of Indianapolis, United States, aiming at in-depth understanding of the spatial patterns of energy fluxes. By computing the fluxes by land use and land cover (LULC) type, we further investigated the spatial variability of heat fluxes. Results show that the energy fluxes possessed a strong seasonality, with the highest net radiation in summer, followed by spring, fall and winter. Sensible heat flux tended to change largely with surface temperature, while latent heat was largely modulated by the change in vegetation abundance and vigor and the accompanying moisture condition. The fluctuation in all heat fluxes tended to be high in the summer months and low in the winter months. Sensible and latent heat fluxes showed a stronger spatial variability than net radiation and ground heat flux. The variations of net radiation among the land use/cover types were mainly attributable to surface albedo and temperature, while the within-class variability in the turbulent heat fluxes was more associated with the changes in vegetation, water bodies, and other surface factors.
C1 [Weng, Qihao] Indiana State Univ, Terre Haute, IN 47809 USA.
   [Hu, Xuefei] Emory Univ, Dept Environm Hlth, Atlanta, GA 30322 USA.
   [Quattrochi, Dale A.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35811 USA.
   [Liu, Hua] Old Dominion Univ, Dept Polit Sci & Geog, Norfolk, VA 23529 USA.
RP Weng, QH (reprint author), Indiana State Univ, Terre Haute, IN 47809 USA.
EM qweng@indstate.edu; xuefei.hu@emory.edu; dale.quattrochi@nasa.gov;
   hxliu@odu.edu
OI Weng, Qihao/0000-0002-2498-0934
FU National Science Foundation [BCS-0521734]; NASA
FX This work was supported by the National Science Foundation under Grant
   BCS-0521734, and a NASA senior fellowship to Q. Weng. (Corresponding
   author: Q. Weng.)
NR 57
TC 9
Z9 9
U1 2
U2 19
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 OCT
PY 2014
VL 7
IS 10
SI SI
BP 4046
EP 4057
DI 10.1109/JSTARS.2013.2281776
PG 12
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
   Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
   Photographic Technology
GA AX5OT
UT WOS:000346977200005
ER

PT J
AU Matsui, T
   Ichoku, C
   Randles, C
   Yuan, T
   da Silva, AM
   Colarco, P
   Kim, D
   Levy, R
   Sayer, A
   Chin, M
   Giles, D
   Holben, B
   Welton, E
   Eck, T
   Remer, L
AF Matsui, Toshi
   Ichoku, Charles
   Randles, Cynthia
   Yuan, Tianle
   da Silva, Arlindo M.
   Colarco, Peter
   Kim, Dongchul
   Levy, Robert
   Sayer, Andrew
   Chin, Mian
   Giles, David
   Holben, Brent
   Welton, Ellsworth
   Eck, Thomas
   Remer, Lorraine
TI CURRENT AND FUTURE PERSPECTIVES OF AEROSOL RESEARCH AT NASA GODDARD
   SPACE FLIGHT CENTER
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
C1 [Matsui, Toshi; Ichoku, Charles; Randles, Cynthia; Yuan, Tianle; da Silva, Arlindo M.; Colarco, Peter; Kim, Dongchul; Levy, Robert; Sayer, Andrew; Chin, Mian; Giles, David; Holben, Brent; Welton, Ellsworth] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Matsui, Toshi] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
   [Randles, Cynthia] Morgan State Univ, Baltimore, MD 21239 USA.
   [Yuan, Tianle; Remer, Lorraine] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
   [Kim, Dongchul; Sayer, Andrew; Eck, Thomas] Univ Space Res Assoc, Columbia, MD USA.
   [Giles, David] Sigma Space Corp, Lanham, MD USA.
RP Matsui, T (reprint author), NASA, Goddard Space Flight Ctr, Mesoscale Dynam & Modeling Grp, Code 612, Greenbelt, MD 20771 USA.
EM toshihisa.matsui-1@nasa.gov
RI Sayer, Andrew/H-2314-2012; Yuan, Tianle/D-3323-2011; Ichoku,
   Charles/E-1857-2012; Kim, Dongchul/H-2256-2012; Levy,
   Robert/M-7764-2013; Chin, Mian/J-8354-2012; Colarco, Peter/D-8637-2012
OI Sayer, Andrew/0000-0001-9149-1789; Ichoku, Charles/0000-0003-3244-4549;
   Kim, Dongchul/0000-0002-5659-1394; Levy, Robert/0000-0002-8933-5303;
   Colarco, Peter/0000-0003-3525-1662
NR 2
TC 0
Z9 0
U1 0
U2 9
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 OCT
PY 2014
VL 95
IS 10
BP ES203
EP ES207
DI 10.1175/BAMS-D-13-00153.1
PG 5
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AW5SZ
UT WOS:000346335400002
ER

PT J
AU Vaishampayan, P
   Roberts, AH
   Augustus, A
   Pukall, R
   Schumann, P
   Schwendner, P
   Mayilraj, S
   Salmassi, T
   Venkateswaran, K
AF Vaishampayan, Parag
   Roberts, Anne Hayden
   Augustus, Angela
   Pukall, Ruediger
   Schumann, Peter
   Schwendner, Petra
   Mayilraj, Shanmugam
   Salmassi, Tina
   Venkateswaran, Kasthuri
TI Deinococcus phoenicis sp nov., an extreme ionizing-radiation-resistant
   bacterium isolated from the Phoenix Lander assembly facility
SO INTERNATIONAL JOURNAL OF SYSTEMATIC AND EVOLUTIONARY MICROBIOLOGY
LA English
DT Article
ID MARS ODYSSEY SPACECRAFT; DIVERSITY; DESERT; SPORES
AB A bacterial strain, designated 1P10ME(T), which was resistant to extreme doses of ionizing radiation, pale-pink, non-motile, and a tetrad-forming coccoid was isolated from a cleanroom at the Kennedy Space Center, where the Phoenix spacecraft was assembled. Strain 1P10ME(T) showed optimum growth at 30 degrees C, with a pH range for growth of 6.5-9.0 and was highly sensitive to sodium chloride, growing only in medium with no added NaCl. Phylogenetic analysis based on 16S rRNA gene sequences indicated that strain 1P10ME(T) represents a novel member of the genus Deinococcus, with low sequence similarities (<93.5 %) to recognized species of the genus Deinococcus. The predominant cellular fatty acid was C-15 : 1 omega 6c. This novel strain exhibits extreme resistance to gamma radiation (D-10 >8 kGy) and UV (D-10 >1000 Jm(-2)). The results of our polyphasic taxonomic analyses suggest that strain 1P10ME(T) represents a novel species of the genus Deinococcus, for which the name Deinococcus phoenicis sp. nov. is proposed. The type strain is 1P10ME(T) (=NRRL B-59546(T)=DSM 27173(T)).
C1 [Vaishampayan, Parag; Venkateswaran, Kasthuri] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA.
   [Roberts, Anne Hayden; Augustus, Angela; Salmassi, Tina] Calif State Univ Los Angeles, Dept Biol Sci, Los Angeles, CA 90032 USA.
   [Pukall, Ruediger; Schumann, Peter] Leibniz Inst DSMZ German Collect Microorganisms &, D-38124 Braunschweig, Germany.
   [Schwendner, Petra] German Aerosp Ctr, Inst Aerosp Med, Cologne, Germany.
   [Mayilraj, Shanmugam] Microbial Type Culture Collect & Gene Bank MTCC, Inst Microbial Technol, Chandigarh 160036, India.
RP Vaishampayan, P (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM vaishamp@jpl.nasa.gov
FU National Aeronautics and Space Administration; NRA ROSES grant; NAI-MIRS
   grant
FX The research described in this publication was carried out at the Jet
   Propulsion Laboratory, California Institute of Technology, under a
   contract with the National Aeronautics and Space Administration. This
   research was funded by a 2007 NRA ROSES grant to K. V. and at California
   State University Los Angeles funded by an NAI-MIRS grant to T. S. The
   authors extend thanks to Shariff Osman and Sudeshna Ghosh for sampling
   and cultivation as well as to Jessica Cisneros (California State
   University, Los Angeles) for technical assistance.
NR 24
TC 1
Z9 1
U1 3
U2 6
PU SOC GENERAL MICROBIOLOGY
PI READING
PA MARLBOROUGH HOUSE, BASINGSTOKE RD, SPENCERS WOODS, READING RG7 1AG,
   BERKS, ENGLAND
SN 1466-5026
EI 1466-5034
J9 INT J SYST EVOL MICR
JI Int. J. Syst. Evol. Microbiol.
PD OCT
PY 2014
VL 64
BP 3441
EP 3446
DI 10.1099/ijs.0.063107-0
PN 10
PG 6
WC Microbiology
SC Microbiology
GA AU8BN
UT WOS:000345821800017
PM 25030518
ER

PT J
AU Naess, S
   Hasselfield, M
   McMahon, J
   Niemack, MD
   Addison, GE
   Ade, PAR
   Allison, R
   Amiri, M
   Battaglia, N
   Beall, JA
   de Bernardis, F
   Bond, JR
   Britton, J
   Calabrese, E
   Cho, HM
   Coughlin, K
   Crichton, D
   Das, S
   Datta, R
   Devlin, MJ
   Dicker, SR
   Dunkley, J
   Dunner, R
   Fowler, JW
   Fox, AE
   Gallardo, P
   Grace, E
   Gralla, M
   Hajian, A
   Halpern, M
   Henderson, S
   Hill, JC
   Hilton, GC
   Hilton, M
   Hincks, AD
   Hlozek, R
   Ho, P
   Hubmayr, J
   Huffenberger, KM
   Hughes, JP
   Infante, L
   Irwin, K
   Jackson, R
   Kasanda, SM
   Klein, J
   Koopman, B
   Kosowsky, A
   Li, D
   Louis, T
   Lungu, M
   Madhavacheril, M
   Marriage, TA
   Maurin, L
   Menanteau, F
   Moodley, K
   Munson, C
   Newburgh, L
   Nibarger, J
   Nolta, MR
   Page, LA
   Pappas, C
   Partridge, B
   Rojas, F
   Schmitt, BL
   Sehgal, N
   Sherwin, BD
   Sievers, J
   Simon, S
   Spergel, DN
   Staggs, ST
   Switzer, ER
   Thornton, R
   Trac, H
   Tucker, C
   Uehara, M
   Van Engelen, A
   Ward, JT
   Wollack, EJ
AF Naess, Sigurd
   Hasselfield, Matthew
   McMahon, Jeff
   Niemack, Michael D.
   Addison, Graeme E.
   Ade, Peter A. R.
   Allison, Rupert
   Amiri, Mandana
   Battaglia, Nick
   Beall, James A.
   de Bernardis, Francesco
   Bond, J. Richard
   Britton, Joe
   Calabrese, Erminia
   Cho, Hsiao-mei
   Coughlin, Kevin
   Crichton, Devin
   Das, Sudeep
   Datta, Rahul
   Devlin, Mark J.
   Dicker, Simon R.
   Dunkley, Joanna
   Duenner, Rolando
   Fowler, Joseph W.
   Fox, Anna E.
   Gallardo, Patricio
   Grace, Emily
   Gralla, Megan
   Hajian, Amir
   Halpern, Mark
   Henderson, Shawn
   Hill, J. Colin
   Hilton, Gene C.
   Hilton, Matt
   Hincks, Adam D.
   Hlozek, Renee
   Ho, Patty
   Hubmayr, Johannes
   Huffenberger, Kevin M.
   Hughes, John P.
   Infante, Leopoldo
   Irwin, Kent
   Jackson, Rebecca
   Kasanda, Simon Muya
   Klein, Jeff
   Koopman, Brian
   Kosowsky, Arthur
   Li, Dale
   Louis, Thibaut
   Lungu, Marius
   Madhavacheril, Mathew
   Marriage, Tobias A.
   Maurin, Loic
   Menanteau, Felipe
   Moodley, Kavilan
   Munson, Charles
   Newburgh, Laura
   Nibarger, John
   Nolta, Michael R.
   Page, Lyman A.
   Pappas, Christine
   Partridge, Bruce
   Rojas, Felipe
   Schmitt, Benjamin L.
   Sehgal, Neelima
   Sherwin, Blake D.
   Sievers, Jon
   Simon, Sara
   Spergel, David N.
   Staggs, Suzanne T.
   Switzer, Eric R.
   Thornton, Robert
   Trac, Hy
   Tucker, Carole
   Uehara, Masao
   Van Engelen, Alexander
   Ward, Jonathan T.
   Wollack, Edward J.
TI The Atacama Cosmology Telescope: CMB polarization at 200 < l < 9000
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE CMBR polarisation; CMBR experiments; cosmological parameters from CMBR;
   CMBR detectors
ID PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND POLARIZATION; SPT-SZ
   SURVEY; POWER SPECTRUM; CRAB-NEBULA; PARAMETERS; CATALOG; MAPS; GHZ;
   CONSTRAINTS
AB We report on measurements of the cosmic microwave background (CMB) and celestial polarization at 146 GHz made with the Atacama Cosmology Telescope Polarimeter (ACTPol) in its first three months of observing. Four regions of sky covering a total of 270 square degrees were mapped with an angular resolution of 1.3'. The map noise levels in the four regions are between 11 and 17 mu K-arcmin. We present TT, TE, EE, TB, EB, and BB power spectra from three of these regions. The observed E-mode polarization power spectrum, displaying six acoustic peaks in the range 200 < l < 3000, is an excellent fit to the prediction of the best-fit cosmological models from WMAP9+ACT and Planck data. The polarization power spectrum, which mainly reflects primordial plasma velocity perturbations, provides an independent determination of cosmological parameters consistent with those based on the temperature power spectrum, which results mostly from primordial density perturbations. We find that without masking any point sources in the EE data at l < 9000, the Poisson tail of the EE power spectrum due to polarized point sources has an amplitude less than 2.4 mu K-2 at l = 3000 at 95% confidence. Finally, we report that the Crab Nebula, an important polarization calibration source at microwave frequencies, has 8.7% polarization with an angle of 150.7 degrees +/- 0.6 degrees when smoothed with a 5' Gaussian beam.
C1 [Naess, Sigurd; Allison, Rupert; Calabrese, Erminia; Dunkley, Joanna] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England.
   [Hasselfield, Matthew; Hill, J. Colin; Hlozek, Renee; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
   [Hasselfield, Matthew; Addison, Graeme E.; Amiri, Mandana; Halpern, Mark; Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
   [McMahon, Jeff; Coughlin, Kevin; Datta, Rahul; Jackson, Rebecca; Munson, Charles] Univ Michigan, Dept Phys, Ann Arbor, MI 48103 USA.
   [Niemack, Michael D.; de Bernardis, Francesco; Gallardo, Patricio; Henderson, Shawn; Koopman, Brian] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
   [Ade, Peter A. R.; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
   [Battaglia, Nick; Trac, Hy] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
   [Beall, James A.; Britton, Joe; Cho, Hsiao-mei; Fowler, Joseph W.; Fox, Anna E.; Hilton, Gene C.; Hubmayr, Johannes; Li, Dale] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
   [Bond, J. Richard; Hajian, Amir; Nolta, Michael R.; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
   [Crichton, Devin; Gralla, Megan; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
   [Das, Sudeep] Argonne Natl Lab, Dept High Energy Phys, Argonne, IL 60439 USA.
   [Devlin, Mark J.; Dicker, Simon R.; Klein, Jeff; Lungu, Marius; Schmitt, Benjamin L.; Ward, Jonathan T.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
   [Duenner, Rolando; Gallardo, Patricio; Infante, Leopoldo; Maurin, Loic; Rojas, Felipe] Pontificia Univ Catolica Chile, Dept Astron & Astrophys, Santiago 22, Chile.
   [Grace, Emily; Ho, Patty; Newburgh, Laura; Page, Lyman A.; Pappas, Christine; Simon, Sara; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
   [Hilton, Matt; Kasanda, Simon Muya; Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
   [Huffenberger, Kevin M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA.
   [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
   [Irwin, Kent] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
   [Jackson, Rebecca] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
   [Kasanda, Simon Muya; Sievers, Jon] Univ KwaZulu Natal, Sch Chem & Phys, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
   [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
   [Madhavacheril, Mathew; Sehgal, Neelima; Van Engelen, Alexander] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
   [Menanteau, Felipe] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
   [Menanteau, Felipe] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
   [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
   [Rojas, Felipe; Uehara, Masao] Sociedad Radiosky Asesoras Ingn Ltd Lincoyan, Concepcion, Chile.
   [Sherwin, Blake D.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA.
   [Sherwin, Blake D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
   [Switzer, Eric R.; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Thornton, Robert] Univ Penn, Dept Phys, W Chester, PA 19383 USA.
RP Naess, S (reprint author), Univ Oxford, Sub Dept Astrophys, Keble Rd, Oxford OX1 3RH, England.
EM sigurd.naess@astro.ox.ac.uk
RI Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012; 
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
   Huffenberger, Kevin/0000-0001-7109-0099; Sievers,
   Jonathan/0000-0001-6903-5074
FU U.S. National Science Foundation [AST-0408698, AST-0965625, PHY-0855887,
   PHY-1214379]; Princeton University; University of Pennsylvania; Canada
   Foundation for Innovation (CFI) award; Comision Nacional de
   Investigacion Cientifica y Tecnologica de Chile (CONICYT); CFI under
   Compute Canada; Government of Ontario; Ontario Research Fund - Research
   Excellence; University of Toronto; NASA [NNX13AE56G, NNX14AB58G,
   NNX12AM32H]; ERC [259505]; NASA ATP [NNX14AB57G]; DOE [DE-SC0011114];
   NSF [AST-1312991]; NASA Space Technology Research Fellowships; CONICYT
   [QUIMAL-120001, FONDECYT-1141113]; Mishrahi Fund; Wilkinson Fund
FX This work was supported by the U.S. National Science Foundation through
   awards AST-0408698 and AST-0965625 for the ACT project, as well as
   awards PHY-0855887 and PHY-1214379. Funding was also provided by
   Princeton University, the University of Pennsylvania, and a Canada
   Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque
   Astronomico Atacama in northern Chile under the auspices of the Comision
   Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT).
   Computations were performed on the GPC supercomputer at the SciNet HPC
   Consortium. SciNet is funded by the CFI under the auspices of Compute
   Canada, the Government of Ontario, the Ontario Research Fund - Research
   Excellence; and the University of Toronto. The development of
   multichroic detectors and lenses was supported by NASA grants NNX13AE56G
   and NNX14AB58G. CM acknowledges support from NASA grant NNX12AM32H.
   Funding from ERC grant 259505 supports SN, JD, EC, and TL. HT is
   supported by grants NASA ATP NNX14AB57G, DOE DE-SC0011114, and NSF
   AST-1312991. BS, BK, CM, and EG are funded by NASA Space Technology
   Research Fellowships. R.D received funding from the CONICYT grants
   QUIMAL-120001 and FONDECYT-1141113. We thank our many colleagues from
   ABS, ALMA, APEX, and POLARBEAR who have helped us at critical junctures.
   Colleagues at AstroNorte and Radio Sky provide logistical support and
   keep operations in Chile running smoothly. We thank Jesse Treu for
   multiple suggestions and comments. We also thank the Mishrahi Fund and
   the Wilkinson Fund for their generous support of the project.
NR 89
TC 55
Z9 55
U1 0
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 OCT
PY 2014
IS 10
AR 007
DI 10.1088/1475-7516/2014/10/007
PG 32
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AW0OA
UT WOS:000345990800008
ER

PT J
AU Ryser, C
   Luthi, MP
   Andrews, LC
   Catania, GA
   Funk, M
   Hawley, R
   Hoffman, M
   Neumann, TA
AF Ryser, C.
   Luethi, M. P.
   Andrews, L. C.
   Catania, G. A.
   Funk, M.
   Hawley, R.
   Hoffman, M.
   Neumann, T. A.
TI Caterpillar-like ice motion in the ablation zone of the Greenland ice
   sheet
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
DE ice dynamics; summer variations; stress transfer
ID JAKOBSHAVN ISBRAE; DRAINAGE SYSTEM; GLACIER MOTION; OUTLET GLACIER;
   SURFACE MELT; BASAL MOTION; DEFORMATION; ACCELERATION; FLOW; DYNAMICS
AB Current understanding of ice dynamics predicts that increasing availability and variability of meltwater will have an impact on basal motion and therefore on the evolution and future behavior of the Greenland ice sheet. We present measurements of ice deformation, subglacial water pressure, and surface velocity that show periodic and episodic variations on several time scales (seasonal, multiday, and diurnal). These variations, observed with GPS and sensors at different depths throughout the ice column, are not synchronous but show delayed responses of ice deformation with increasing depth and basal water pressure in antiphase with surface velocity. With the help of a Full-Stokes ice flow model, these observations are explained as ice motion in a caterpillar-like fashion. Caused by patches of different basal slipperiness, horizontal stress transfer through the stiff central part of the ice body leads to spatially varying surface velocities and ice deformation patterns. Variation of this basal slipperiness induces characteristic patterns of ice deformation variability that explain the observed behavior. Ice flow in the ablation zone of the Greenland ice sheet is therefore controlled by activation of basal patches by varying slipperiness in the course of a melt season, leading to caterpillar-like ice motion superposed on the classical shear deformation.
C1 [Ryser, C.; Luethi, M. P.; Funk, M.] ETH, Versuchsanstalt Wasserbau Hydrol & Glaziol, Zurich, Switzerland.
   [Andrews, L. C.; Catania, G. A.] Univ Texas Austin, Inst Geophys, Austin, TX USA.
   [Andrews, L. C.; Catania, G. A.] Univ Texas Austin, Dept Geol Sci, Austin, TX USA.
   [Hawley, R.] Dartmouth Coll, Dept Earth Sci, Hanover, NH 03755 USA.
   [Hoffman, M.] Los Alamos Natl Lab, Fluid Dynam & Solid Mech Grp, Los Alamos, NM USA.
   [Neumann, T. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ryser, C (reprint author), ETH, Versuchsanstalt Wasserbau Hydrol & Glaziol, Zurich, Switzerland.
EM ryser@vaw.baug.ethz.ch
RI Catania, Ginny/B-9787-2008; Neumann, Thomas/D-5264-2012; Andrews,
   Lauren/D-8274-2017; 
OI Andrews, Lauren/0000-0003-3727-4737; Luthi, Martin
   Peter/0000-0003-4419-8496
FU Swiss National Science Foundation [200021_127197]; US-NSF [OPP 0908156,
   OPP 0909454, ANT-0424589]; NASA Cryospheric Sciences; Climate Modeling
   Programs within the U.S. Department of Energy Office of Science
FX We thank several people who were essential in this project: Cornelius
   Senn, Edi Imhof, Thomas Wyder, Andreas Bauder, Christian Birchler,
   Michael Meier, Blaine Moriss, and Fabian Walter. This project was
   supported by Swiss National Science Foundation grant 200021_127197;
   US-NSF grants OPP 0908156, OPP 0909454, and ANT-0424589 (to CRe-SIS);
   NASA Cryospheric Sciences; and Climate Modeling Programs within the U.S.
   Department of Energy Office of Science. Logistical support was provided
   by CH2MHill Polar Services. GPS receivers were provided by UNAVCO. We
   thank "Microwave and Remote Sensing, DTU Space, the Technical University
   of Denmark" for providing bedrock topography data of the area. We also
   acknowledge the help of pilots and airport cargo staff of Air Greenland
   in Ilulissat. Further, we thank Jason Gulley and Martin Truffer for
   commenting on the manuscript. We acknowledge the reviews by David
   Podrasky, two anonymous referees, and scientific Editor Bryn Hubbard.
NR 45
TC 12
Z9 12
U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9003
EI 2169-9011
J9 J GEOPHYS RES-EARTH
JI J. Geophys. Res.-Earth Surf.
PD OCT
PY 2014
VL 119
IS 10
BP 2258
EP 2271
DI 10.1002/2013JF003067
PG 14
WC Geosciences, Multidisciplinary
SC Geology
GA AU1FN
UT WOS:000345366600009
ER

PT J
AU Vernieres, G
   Kovach, R
   Keppenne, C
   Akella, S
   Brucker, L
   Dinnat, E
AF Vernieres, G.
   Kovach, R.
   Keppenne, C.
   Akella, S.
   Brucker, L.
   Dinnat, E.
TI The impact of the assimilation of Aquarius sea surface salinity data in
   the GEOS ocean data assimilation system
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE data assimilation; aquarius; salinity; neural network
ID ENSEMBLE KALMAN FILTER; NEURAL-NETWORKS; MODEL; TEMPERATURE; CLIMATE;
   RAIN; SMOS
AB Ocean salinity and temperature differences drive thermohaline circulation. These properties also play a key role in the ocean-atmosphere coupling. With the availability of L-band space-borne observations, it becomes possible to provide global scale sea surface salinity (SSS) distribution. This study analyzes globally the along-track (Level 2) Aquarius SSS retrievals obtained using both passive and active L-band observations. Aquarius along-track retrieved SSS are assimilated into the ocean data assimilation component of Version 5 of the Goddard Earth Observing System (GEOS-5) assimilation and forecast model. We present a methodology to correct the large biases and errors apparent in Version 2.0 of the Aquarius SSS retrieval algorithm and map the observed Aquarius SSS retrieval into the ocean model's bulk salinity in the topmost layer. The impact of the assimilation of the corrected SSS on the salinity analysis is evaluated by comparisons with in situ salinity measurements from Argo. The results show a significant reduction of the global biases and RMS of observations-minus-forecast differences at in situ locations. The most striking results are found in the tropics and southern latitudes. Our results highlight the complementary role and problems that arise during the assimilation of salinity information from in situ (Argo) and space-borne SSS retrievals.
C1 [Vernieres, G.; Kovach, R.; Keppenne, C.; Akella, S.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
   [Vernieres, G.; Kovach, R.; Keppenne, C.; Akella, S.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
   [Brucker, L.; Dinnat, E.] NASA, GSFC, Cryospher Sci Lab, Greenbelt, MD USA.
   [Brucker, L.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Columbia, MD USA.
   [Dinnat, E.] Chapman Univ, Ctr Excellence Earth Syst Modeling & Observat, Orange, CA USA.
RP Vernieres, G (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM guillaume.vernieres-1@nasa.gov
RI Dinnat, Emmanuel/D-7064-2012; Brucker, Ludovic/A-8029-2010
OI Dinnat, Emmanuel/0000-0001-9003-1182; Brucker,
   Ludovic/0000-0001-7102-8084
FU NASA's Modeling Analysis and Prediction Program [WBS 802678.02.17.01.25]
FX This work was supported by NASA's Modeling Analysis and Prediction
   Program under WBS 802678.02.17.01.25. The computational resources for
   the runs were provided by the NASA Center for Climate Simulation (NCCS).
   Yuri Vikhliaev, Max Suarez, and Bin Zhao of GMAO integrated MOM4 and
   CICE into the GEOS-5 modeling system and configured the system used in
   this study. Their support is gratefully acknowledged. The authors would
   also like to thank Michele Rienecker and the two anonymous reviewers for
   their many insightful comments.
NR 37
TC 4
Z9 4
U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD OCT
PY 2014
VL 119
IS 10
BP 6974
EP 6987
DI 10.1002/2014JC010006
PG 14
WC Oceanography
SC Oceanography
GA AU3GF
UT WOS:000345499700026
ER

PT J
AU Kim, SB
   Lee, JH
   de Matthaeis, P
   Yueh, S
   Hong, CS
   Lee, JH
   Lagerloef, G
AF Kim, Seung-bum
   Lee, Jae Hak
   de Matthaeis, Paolo
   Yueh, Simon
   Hong, Chang-Su
   Lee, Joon-Ho
   Lagerloef, Gary
TI Sea surface salinity variability in the East China Sea observed by the
   Aquarius instrument
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE salinity; remote sensing
ID SOIL-MOISTURE; OCEAN; ERROR; RIVER; SMOS
AB This study demonstrates that the spaceborne Aquarius instrument is able to monitor the sea surface salinity (SSS) variations in the East China Sea (ECS) with the spatial resolution of about 150 km at 7 day interval, where routine observations are difficult. The two geophysical contaminants enter the sidelobes of the Aquarius antenna and bias the coastal SSS low: the emission from the land surface and the radiofrequency interference (RFI). Away from about one Aquarius pixel (150 km) from the coastline, the Aquarius SSS is fairly insensitive (less than about 0.2 psu) to the radiometric details of the method to correct for the land emission. The ascending orbits appear to be affected by unfiltered RFI much less than the descending tracks. The Aquarius SSS along the ascending tracks is low over the ECS by 0.40-0.93 psu (with respect to the in situ data during the two separate 7 day periods) and is biased low by 0.41-1.07 psu (accuracy, or the time-mean of difference from the regional model along three Aquarius tracks over a 18 month period). The presence of the ascending and descending differences in the Aquarius SSS, and the spatially widespread bias suggest that the bias is attributed to the unfiltered RFI originating from strong point sources (rather than to the land contamination from weak distributed sources, or to other seasonally varying geophysical contaminants). Despite the bias, the Aquarius data describe well the temporal and spatial variability of the ECS SSS. The temporal trend and magnitude of salinity changes agree remarkably between Aquarius and a regional numerical model, during both the freshwater discharge season from the Yangtze river and the rest of the year. The precision of the Aquarius observation in the ECS is comparable with the Aquarius mission requirement (0.2 psu one-sigma for a monthly average over the open ocean). The river discharge rate correlates with the Aquarius SSS with the coefficient of 0.71 on a seasonal scale with the discharge leading the SSS changes. The Aquarius SSS increases away from the coast, in response to the river outflow. The interannual changes in the Aquarius SSS capture the effect of the regional drought in summer 2013.
C1 [Kim, Seung-bum; Yueh, Simon] CALTECH, Jet Prop Lab, Dept Earth & Marine Sci, Pasadena, CA 91125 USA.
   [Lee, Jae Hak; Hong, Chang-Su] Korea Inst Ocean Sci & Technol, Dept Earth & Marine Sci, Ansan, South Korea.
   [de Matthaeis, Paolo] NASA, Goddard Space Flight Ctr, Dept Earth & Marine Sci, Greenbelt, MD 20771 USA.
   [Lee, Joon-Ho] Jeju Natl Univ, Dept Earth & Marine Sci, Cheju, South Korea.
   [Lagerloef, Gary] Earth & Space Res, Dept Earth & Marine Sci, Seattle, WA USA.
RP Kim, SB (reprint author), CALTECH, Jet Prop Lab, Dept Earth & Marine Sci, Pasadena, CA 91125 USA.
EM Seungbum.Kim@jpl.nasa.gov
FU National Aeronautics and Space Administration; National Research
   Foundation of Korea Grant - South Korean Government
   [NRF-2009-C1AAA001-0093065]
FX The comments by two reviewers were very helpful to significantly improve
   the manuscript. We thank Steven Riser for valuable discussions. The MWR
   rain rate retrieval data were provided by J. Scott, Remote Sensing
   Systems, USA. This research was carried out in part at the Jet
   Propulsion Laboratory, California Institute of Technology, under a
   contract with the National Aeronautics and Space Administration. Jae Hak
   Lee and Chang-Su Hong were supported by the National Research Foundation
   of Korea Grant funded by the South Korean Government
   (NRF-2009-C1AAA001-0093065).
NR 24
TC 4
Z9 5
U1 2
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD OCT
PY 2014
VL 119
IS 10
BP 7016
EP 7028
DI 10.1002/2014JC009983
PG 13
WC Oceanography
SC Oceanography
GA AU3GF
UT WOS:000345499700029
ER

PT J
AU Hijazi, H
   Bannister, ME
   Meyer, HM
   Rouleau, CM
   Barghouty, AF
   Rickman, DL
   Meyer, FW
AF Hijazi, H.
   Bannister, M. E.
   Meyer, H. M., III
   Rouleau, C. M.
   Barghouty, A. F.
   Rickman, D. L.
   Meyer, F. W.
TI Anorthite sputtering by H+ and Arq+ (q=1-9) at solar wind velocities
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE solar wind; lunar highlands; sputtering; ion-surface interactions
ID QUARTZ-CRYSTAL MICROBALANCE; HIGHLY-CHARGED IONS; DECELERATED BEAMS;
   ENERGY-DEPENDENCE; LUNAR POLES; SURFACE; ORNL; HYDROGEN; IMPACT; YIELD
AB We report sputtering measurements of anorthite-like material, taken to be representative of soils found in the lunar highlands, impacted by singly and multicharged ions representative of the solar wind. The ions investigated include protons, as well as singly and multicharged Ar ions (as proxies for the nonreactive heavy solar wind constituents), in the charge state range +1 to +9, at fixed solar wind-relevant impact velocities of 165 and 310km/s (0.25keV/amu and 0.5keV/amu). A quartz microbalance approach (QCM) for determination of total sputtering yields was used. The goal of the measurements was to determine the sputtering contribution of the heavy, multicharged minority solar wind constituents in comparison to that due to the dominant H+ fraction. The QCM results show a yield increase of a factor of about 80 for Ar+ versus H+ sputtering and an enhancement by a factor of 1.67 between Ar9+ and Ar+, which is a clear indication of a potential sputtering effect.
C1 [Hijazi, H.; Bannister, M. E.; Meyer, F. W.] Oak Ridge Natl Lab, Div Phys, Oak Ridge, TN 37831 USA.
   [Meyer, H. M., III] Oak Ridge Natl Lab, Mat Sci & Technol Div, Oak Ridge, TN 37831 USA.
   [Rouleau, C. M.] Oak Ridge Natl Lab, Ctr Nanophase Mat Sci, Oak Ridge, TN 37831 USA.
   [Barghouty, A. F.; Rickman, D. L.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Meyer, FW (reprint author), Oak Ridge Natl Lab, Div Phys, Oak Ridge, TN 37831 USA.
EM meyerfw@ornl.gov
RI Rouleau, Christopher/Q-2737-2015
OI Rouleau, Christopher/0000-0002-5488-3537
FU NASA [10-LASER10-0053]; Laboratory Directed Research and Development
   Program of Oak Ridge National Laboratory; NASA's Solar System
   Exploration Research Institute (SSERVI); Office of Basic Energy
   Sciences, U.S. Department of Energy; Scientific User Facilities (SUF)
   Division, U.S. Department of Energy
FX Research supported by NASA grant 10-LASER10-0053, by the Laboratory
   Directed Research and Development Program of Oak Ridge National
   Laboratory, managed by UT-Battelle, LLC, for the U.S. Department of
   Energy, and in part by NASA's Solar System Exploration Research
   Institute (SSERVI). Work performed in part via ORNL's Shared Research
   Equipment (ShaRE) User Program, which is sponsored by the Office of
   Basic Energy Sciences, U.S. Department of Energy, and at the Center for
   Nanophase Materials Sciences user facility, which is sponsored at Oak
   Ridge National Laboratory by the Scientific User Facilities (SUF)
   Division, U.S. Department of Energy. H. H. was appointed through the
   ORNL Postdoctoral Research Associates Program administered jointly by
   Oak Ridge Institute of Science and Education (ORISE), Oak Ridge
   Associated Universities (ORAU), and Oak Ridge National Laboratory
   (ORNL). The data for this paper can be requested from meyerfw@ornl.gov
   (F.W. Meyer).
NR 34
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 OCT
PY 2014
VL 119
IS 10
BP 8006
EP 8016
DI 10.1002/2014JA020140
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AU2JW
UT WOS:000345445400003
ER

PT J
AU Boardsen, SA
   Adrian, ML
   Pfaff, R
   Menietti, JD
AF Boardsen, S. A.
   Adrian, M. L.
   Pfaff, R.
   Menietti, J. D.
TI Inner magnetospheric electron temperature and spacecraft potential
   estimated from concurrent Polar upper hybrid frequency and relative
   potential measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE current balance; electron temperature; upper hybrid frequency; probe
   potential; spacecraft potential
ID PLASMA-DENSITY; EARTHS MAGNETOSPHERE; GEOTAIL SPACECRAFT; PROBE
   MEASUREMENTS; FIELD ANTENNAS; AURORAL-ZONE; SATELLITE; PHOTOEMISSION;
   INSTRUMENT; DEPENDENCE
AB Direct measurement of low <1eV electron temperature is difficult to make in the Earth's inner magnetosphere for electron densities (N-e)<3x10(2) cm(-3). We compute these quantities by solving current balance equations in low-density regions. Concurrent measurements from the Polar spacecraft of the relative potential (V-S-V-P), between the spacecraft body and the electric field probe, and the electron density (N-e), derived from upper hybrid frequency (f(UHR)), were used in the current balance equations to solve for the electron temperature (T-e), V-s, and V-p. Where V-P is the probe potential and V-S is the spacecraft potential relative to the nearby plasma. The assumption that the bulk plasma electrons are Maxwellian is used in the computations. Our data set covered 1.5years of measurements when f(UHR) was detectable (L<10). The following averaged T-e versus L relation for 3<L<5 was obtained: T-e=0.58+0.49(L-3)eV. This expression is in reasonable agreement with extrapolations of ionospheric T-e measurements by Akebono at lower altitudes. However, the solution is sensitive to the photoemission coefficients, substituting those of Scudder et al. (2000) with those of Escoubet et al. (1997), the T-e curve shifted upward by similar to 1eV. Also, the solution is sensitive to measurement error of V-S-V-P, applying a voltage shift of 0.1 and 0.2V to V-S-V-P, the relative median error for our data set was computed to be 0.27 and 1.04, respectively. We believe that our T-e values computed outside the plasmasphere are unrealistically low. We conclude that this method shows promise inside the plasmasphere but should be used with caution. We also quantified the N-e versus V-S-V-P relationship. The running median N-e versus V-S-V-P curve shows no significant variation over the 1.5year period of the data set, suggesting that the photoemission coefficients did not change significantly over this time span. The Scudder et al. (2000) N-e model, based on only one Polar orbit, is in reasonable agreement (within a factor of 2) with our results.
C1 [Boardsen, S. A.] Univ Maryland, Goddard Planetary & Heliophys Inst, Baltimore, MD 21201 USA.
   [Boardsen, S. A.; Adrian, M. L.; Pfaff, R.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA.
   [Menietti, J. D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
RP Boardsen, SA (reprint author), Univ Maryland, Goddard Planetary & Heliophys Inst, Baltimore, MD 21201 USA.
EM Scott.A.Boardsen@nasa.gov
NR 43
TC 0
Z9 0
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD OCT
PY 2014
VL 119
IS 10
BP 8046
EP 8062
DI 10.1002/2014JA019852
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AU2JW
UT WOS:000345445400006
ER

PT J
AU Slavin, JA
   DiBraccio, GA
   Gershman, DJ
   Imber, SM
   Poh, GK
   Raines, JM
   Zurbuchen, TH
   Jia, XZ
   Baker, DN
   Glassmeier, KH
   Livi, SA
   Boardsen, SA
   Cassidy, TA
   Sarantos, M
   Sundberg, T
   Masters, A
   Johnson, CL
   Winslow, RM
   Anderson, BJ
   Korth, H
   McNutt, RL
   Solomon, SC
AF Slavin, James A.
   DiBraccio, Gina A.
   Gershman, Daniel J.
   Imber, Suzanne M.
   Poh, Gang Kai
   Raines, Jim M.
   Zurbuchen, Thomas H.
   Jia, Xianzhe
   Baker, Daniel N.
   Glassmeier, Karl-Heinz
   Livi, Stefano A.
   Boardsen, Scott A.
   Cassidy, Timothy A.
   Sarantos, Menelaos
   Sundberg, Torbjorn
   Masters, Adam
   Johnson, Catherine L.
   Winslow, Reka M.
   Anderson, Brian J.
   Korth, Haje
   McNutt, Ralph L.
   Solomon, Sean C.
TI MESSENGER observations of Mercury's dayside magnetosphere under extreme
   solar wind conditions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Mercury; magnetosphere; reconnection; cusp; plasma depletion layer; core
   induction
ID FLUX-TRANSFER EVENTS; INTERPLANETARY MAGNETIC-FIELD; POLAR CUSP;
   MAGNETOPAUSE OBSERVATIONS; EARTHS MAGNETOPAUSE; RECONNECTION RATE;
   PLASMA DEPLETION; BOW SHOCKS; 1ST FLYBY; EXOSPHERE
AB The structure of Mercury's dayside magnetosphere is investigated during three extreme solar wind dynamic pressure events. Two were the result of coronal mass ejections (CMEs), and one was from a high-speed stream (HSS). The inferred pressures for these events are similar to 45 to 65 nPa. The CME events produced thick, low- (where is the ratio of plasma thermal to magnetic pressure) plasma depletion layers and high reconnection rates of 0.1-0.2, despite small magnetic shear angles across the magnetopause of only 27 to 60 degrees. For one of the CME events, brief, similar to 1-2 s long diamagnetic decreases, which we term cusp plasma filaments, were observed within and adjacent to the cusp. These filaments may map magnetically to flux transfer events at the magnetopause. The HSS event produced a high- magnetosheath with no plasma depletion layer and large magnetic shear angles of 148 to 166 degrees, but low reconnection rates of 0.03 to 0.1. These results confirm that magnetic reconnection at Mercury is very intense, and its rate is primarily controlled by plasma in the adjacent magnetosheath. The distance to the subsolar magnetopause is reduced during these events from its mean of 1.45 Mercury radii (R-M) from the planetary magnetic dipole to between 1.03 and 1.12 R-M. The shielding provided by induction currents in Mercury's interior, which temporarily increase Mercury's magnetic moment, was negated by reconnection-driven magnetic flux erosion.
C1 [Slavin, James A.; DiBraccio, Gina A.; Gershman, Daniel J.; Imber, Suzanne M.; Poh, Gang Kai; Raines, Jim M.; Zurbuchen, Thomas H.; Jia, Xianzhe] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
   [Gershman, Daniel J.; Boardsen, Scott A.; Sarantos, Menelaos] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA.
   [Imber, Suzanne M.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
   [Baker, Daniel N.; Cassidy, Timothy A.] Univ Colorado, Lab Solar & Atmospher Phys, Boulder, CO 80309 USA.
   [Glassmeier, Karl-Heinz] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, Braunschweig, Germany.
   [Livi, Stefano A.] SW Res Inst, San Antonio, TX USA.
   [Boardsen, Scott A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
   [Sarantos, Menelaos] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
   [Sundberg, Torbjorn] Queen Mary Univ London, Sch Phys & Astron, London, England.
   [Masters, Adam] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London, England.
   [Johnson, Catherine L.; Winslow, Reka M.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V5Z 1M9, Canada.
   [Johnson, Catherine L.; Winslow, Reka M.] Planetary Sci Inst, Tucson, AZ USA.
   [Anderson, Brian J.; Korth, Haje; McNutt, Ralph L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
   [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DE USA.
   [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
RP Slavin, JA (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM jaslavin@umich.edu
RI Jia, Xianzhe/C-5171-2012; McNutt, Ralph/E-8006-2010; Poh,
   Gangkai/O-5378-2016; Slavin, James/H-3170-2012
OI Jia, Xianzhe/0000-0002-8685-1484; McNutt, Ralph/0000-0002-4722-9166;
   Poh, Gangkai/0000-0002-5775-2006; Slavin, James/0000-0002-9206-724X
FU Natural Sciences and Engineering Research Council of Canada; MESSENGER
   Participating Scientist grant [NNX11AB84G]; NASA [NASW-00002,
   NAS5-97271]
FX We gratefully acknowledge the contribution of WSA-ENLIL simulations and
   graphic displays provided by P. J. Macneice and M. L. Mays of the
   Community Coordinated Modeling Center at the NASA Goddard Space Flight
   Center. Discussions with J. L. Burch concerning plasma injection into
   Earth's cusps are also acknowledged. CLJ and RMW acknowledge support
   from the Natural Sciences and Engineering Research Council of Canada,
   and CLJ acknowledges support from MESSENGER Participating Scientist
   grant NNX11AB84G. 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.
NR 121
TC 24
Z9 24
U1 1
U2 16
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 OCT
PY 2014
VL 119
IS 10
BP 8087
EP 8116
DI 10.1002/2014JA020319
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AU2JW
UT WOS:000345445400009
ER

PT J
AU Hartinger, MD
   Welling, D
   Viall, NM
   Moldwin, MB
   Ridley, A
AF Hartinger, M. D.
   Welling, D.
   Viall, N. M.
   Moldwin, M. B.
   Ridley, A.
TI The effect of magnetopause motion on fast mode resonance
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE ULF wave; fast mode resonance; magnetopause; MHD wave; cavity mode;
   global mode
ID MAGNETOSPHERIC WAVE-GUIDE; MAGNETIC-FIELD; ULF PULSATIONS; DIPOLE
   MAGNETOSPHERE; CAVITY MODES; SPACECRAFT; MAGNETOHYDRODYNAMICS;
   ACCELERATION; OSCILLATIONS; WIND
AB The Earth's magnetosphere supports several types of ultralow frequency (ULF) waves. These include fast mode resonance (FMR): cavity modes, waveguide modes, and tunneling modes/virtual resonance. The magnetopause, often treated as the outer boundary for cavity/waveguide modes in the dayside magnetosphere, is not stationary. A rapidly changing outer boundary conditione.g., due to rapid magnetopause motionis not favorable for FMR generation and may explain the sparseness of FMR observations in the outer magnetosphere. We examine how magnetopause motion affects the dayside magnetosphere's ability to sustain FMR with idealized Space Weather Modeling Framework (SWMF) simulations using the BATS-R-US global magnetohydrodynamic (MHD) code coupled with the Ridley Ionosphere Model (RIM). We present observations of FMR in BATS-R-US, reproducing results from other global MHD codes. We further show that FMR is present for a wide range of solar wind conditions, even during periods with large and rapid magnetopause displacements. We compare our simulation results to FMR observations in the dayside magnetosphere, finding that FMR occurrence does not depend on solar wind dynamic pressure, which can be used as a proxy for dynamic pressure fluctuations and magnetopause perturbations. Our results demonstrate that other explanations besides a nonstationary magnetopausesuch as the inability to detect FMR in the presence of other ULF wave modes with large amplitudesare required to explain the rarity of FMR observations in the outer magnetosphere.
C1 [Hartinger, M. D.; Welling, D.; Moldwin, M. B.; Ridley, A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
   [Viall, N. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hartinger, MD (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM mdhartin@umich.edu
RI Hartinger, Michael/H-9088-2012; Moldwin, Mark/F-8785-2011; Ridley,
   Aaron/F-3943-2011
OI Hartinger, Michael/0000-0002-2643-2202; Moldwin,
   Mark/0000-0003-0954-1770; Ridley, Aaron/0000-0001-6933-8534
FU NSF [AGS-1230398]; National Science Foundation [ACI-1053575]
FX We thank S. G. Claudepierre, M. Wiltberger, and M. G. Kivelson for
   helpful discussions and suggestions. We also thank the NASA Space
   Science Data facility for use of solar wind data. M. D. Hartinger was
   funded through NSF grant AGS-1230398. We would like to acknowledge
   high-performance computing support from Yellowstone
   (ark:/85065/d7wd3xhc) provided by NCAR's Computational and Information
   Systems Laboratory, sponsored by the National Science Foundation. We
   also acknowledge the Extreme Science and Engineering Discovery
   Environment (XSEDE), which is supported by National Science Foundation
   grant ACI-1053575. This work was carried out using the SWMF/BATSRUS
   tools developed at the University of Michigan Center for Space
   Environment Modeling (CSEM). Simulation output files are available upon
   request from the corresponding author (M. D. Hartinger,
   mdhartin@umich.edu). The authors thank Kazue Takahashi and Scott
   Boardsen for their comments.
NR 47
TC 4
Z9 4
U1 1
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 OCT
PY 2014
VL 119
IS 10
BP 8212
EP 8227
DI 10.1002/2014JA020401
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AU2JW
UT WOS:000345445400017
ER

PT J
AU Fu, XR
   Cowee, MM
   Friedel, RH
   Funsten, HO
   Gary, SP
   Hospodarsky, GB
   Kletzing, C
   Kurth, W
   Larsen, BA
   Liu, KJ
   MacDonald, EA
   Min, K
   Reeves, GD
   Skoug, RM
   Winske, D
AF Fu, Xiangrong
   Cowee, Misa M.
   Friedel, Reinhard H.
   Funsten, Herbert O.
   Gary, S. Peter
   Hospodarsky, George B.
   Kletzing, Craig
   Kurth, William
   Larsen, Brian A.
   Liu, Kaijun
   MacDonald, Elizabeth A.
   Min, Kyungguk
   Reeves, Geoffrey D.
   Skoug, Ruth M.
   Winske, Dan
TI Whistler anisotropy instabilities as the source of banded chorus: Van
   Allen Probes observations and particle-in-cell simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE chorus; particle-in-cell simulation; HOPE; Van Allen Probes
ID RADIATION-BELT ELECTRONS; MAGNETOSPHERIC CHORUS; ACCELERATION; WAVES;
   EMISSIONS
AB Magnetospheric banded chorus is enhanced whistler waves with frequencies (r)<(e), where (e) is the electron cyclotron frequency, and a characteristic spectral gap at (r)similar or equal to(e)/2. This paper uses spacecraft observations and two-dimensional particle-in-cell simulations in a magnetized, homogeneous, collisionless plasma to test the hypothesis that banded chorus is due to local linear growth of two branches of the whistler anisotropy instability excited by two distinct, anisotropic electron components of significantly different temperatures. The electron densities and temperatures are derived from Helium, Oxygen, Proton, and Electron instrument measurements on the Van Allen Probes A satellite during a banded chorus event on 1 November 2012. The observations are consistent with a three-component electron model consisting of a cold (a few tens of eV) population, a warm (a few hundred eV) anisotropic population, and a hot (a few keV) anisotropic population. The simulations use plasma and field parameters as measured from the satellite during this event except for two numbers: the anisotropies of the warm and the hot electron components are enhanced over the measured values in order to obtain relatively rapid instability growth. The simulations show that the warm component drives the quasi-electrostatic upper band chorus and that the hot component drives the electromagnetic lower band chorus; the gap at approximate to(e)/2 is a natural consequence of the growth of two whistler modes with different properties.
C1 [Fu, Xiangrong; Cowee, Misa M.; Friedel, Reinhard H.; Funsten, Herbert O.; Larsen, Brian A.; Reeves, Geoffrey D.; Skoug, Ruth M.; Winske, Dan] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
   [Gary, S. Peter] Space Sci Inst, Boulder, CO USA.
   [Hospodarsky, George B.; Kletzing, Craig; Kurth, William] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
   [Liu, Kaijun; Min, Kyungguk] Auburn Univ, Dept Phys, Auburn, AL 36849 USA.
   [MacDonald, Elizabeth A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Fu, XR (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
EM xrfu@lanl.gov
RI Larsen, Brian/A-7822-2011; Fu, Xiangrong/C-7895-2016; Reeves,
   Geoffrey/E-8101-2011; Funsten, Herbert/A-5702-2015; Friedel,
   Reiner/D-1410-2012
OI Larsen, Brian/0000-0003-4515-0208; Fu, Xiangrong/0000-0002-4305-6624;
   Reeves, Geoffrey/0000-0002-7985-8098; Kletzing,
   Craig/0000-0002-4136-3348; Hospodarsky, George/0000-0001-9200-9878;
   Kurth, William/0000-0002-5471-6202; Funsten,
   Herbert/0000-0002-6817-1039; Friedel, Reiner/0000-0002-5228-0281
FU U.S. Department of Energy; Defense Threat Reduction Agency; National
   Aeronautics and Space Administration; National Science Foundation;
   JHU/APL under NASA [921647, NAS5-01072]; NSF [AGS-1303300]; NASA
   [NNX14AD62G]
FX The Los Alamos portion of this research was performed under the auspices
   of the U.S. Department of Energy. This research was supported in part by
   the Defense Threat Reduction Agency, by the National Aeronautics and
   Space Administration, and by the National Science Foundation. The work
   at the University of Iowa was supported by JHU/APL through contract
   921647 under NASA Prime contract NAS5-01072. S.P.G.'s contributions to
   this research were supported by NSF award AGS-1303300. The work at
   Auburn University was supported by NASA grant NNX14AD62G.
NR 32
TC 25
Z9 25
U1 0
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD OCT
PY 2014
VL 119
IS 10
BP 8288
EP 8298
DI 10.1002/2014JA020364
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AU2JW
UT WOS:000345445400023
ER

PT J
AU Garcia, RA
   McKinna, LIW
   Hedley, JD
   Fearns, PRCS
AF Garcia, Rodrigo A.
   McKinna, Lachlan I. W.
   Hedley, John D.
   Fearns, Peter R. C. S.
TI Improving the optimization solution for a semi-analytical shallow water
   inversion model in the presence of spectrally correlated noise
SO LIMNOLOGY AND OCEANOGRAPHY-METHODS
LA English
DT Article
ID INHERENT OPTICAL-PROPERTIES; REMOTE-SENSING REFLECTANCE; OCEAN COLOR;
   WESTERN-AUSTRALIA; SHARK BAY; RETRIEVAL; ALGORITHM; LIMITATIONS; SPACE;
   DEEP
AB In coastal regions, shallow water semi-analytical inversion algorithms may be used to derive geophysical parameters such as inherent optical properties (IOPs), water column depth, and bottom albedo coefficients by inverting sensor-derived sub-surface remote sensing reflectance, r(rs). The uncertainties of these derived geophysical parameters due to instrumental and environmental noise can be estimated numerically via the addition of spectral noise to the sensor-derived r(rs) before inversion. Repeating this process multiple times allows the calculation of the standard error and average for each derived parameter. Apart from spectral non-uniqueness, the optimization algorithm employed in the inversion must converge onto a single minimum to obtain a true representation of the uncertainty for a given set of noise-perturbed r(rs). Failure to do so inflates the uncertainty and affects the average retrieved value (accuracy). We show that the standard approach of seeding the optimization with an arbitrary, fixed initial guess, can lead to the convergence to multiple minima, each having substantially different centroids in multi-parameter solution space. We present the Update-Repeat Levenberg-Marquardt (UR-LM) and Latin Hypercube Sampling (LHS) routines that dynamically search the solution space for an optimal initial guess, that when applied to the optimization allows convergence to the best local minimum. We apply the UR-LM and LHS methods on HICO-derived and simulated r(rs) and demonstrate the improved computational efficiency, precision, and accuracy afforded from these methods compared with the standard approach. Conceptually, these methods are applicable to remote sensing based, shallow water or oceanic semi-analytical inversion algorithms requiring nonlinear least squares optimization.
C1 [Garcia, Rodrigo A.; McKinna, Lachlan I. W.; Fearns, Peter R. C. S.] Curtin Univ, Dept Imaging & Appl Phys, Remote Sensing & Satellite Res Grp, Perth, WA 6845, Australia.
   [McKinna, Lachlan I. W.] Goddard Space Flight Ctr, Ocean Ecol Lab, NASA Postdoctoral Program Fellow, Greenbelt, MD 20771 USA.
   [Hedley, John D.] Environm Comp Sci Ltd, Tiverton EX16 6LR, Devon, England.
RP Garcia, RA (reprint author), Curtin Univ, Dept Imaging & Appl Phys, Remote Sensing & Satellite Res Grp, GPO Box U1987, Perth, WA 6845, Australia.
EM rodrigo.garcia@postgrad.curtin.edu.au
FU Australian Postgraduate Award
FX This research was supported by an Australian Postgraduate Award
   administered by Curtin University. The authors would like to thank Dr.
   Craig Markwardt for his valued advice regarding the MPFIT implementation
   of the Levenberg-Marquardt optimization routine. The authors also thank
   the HICO project team at both OSU and NRL for targeting, processing, and
   distribution of HICO L1B data over Shark Bay. All HICO T data were
   provided by the Naval Research Laboratory through the Oregon State
   University, College of Earth, Ocean, and Atmospheric Sciences' HICO
   website (hico.coas.oregonstate.edu).
NR 32
TC 3
Z9 3
U1 1
U2 7
PU AMER SOC LIMNOLOGY OCEANOGRAPHY
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA
SN 1541-5856
J9 LIMNOL OCEANOGR-METH
JI Limnol. Oceanogr. Meth.
PD OCT
PY 2014
VL 12
BP 651
EP 669
DI 10.4319/lom.2014.12.651
PG 19
WC Limnology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA AU0XW
UT WOS:000345346500001
ER

PT J
AU Lestari, RK
   Watanabe, M
   Imada, Y
   Shiogama, H
   Field, RD
   Takemura, T
   Kimoto, M
AF Lestari, R. Kartika
   Watanabe, Masahiro
   Imada, Yukiko
   Shiogama, Hideo
   Field, Robert D.
   Takemura, Toshihiko
   Kimoto, Masahide
TI Increasing potential of biomass burning over Sumatra, Indonesia induced
   by anthropogenic tropical warming
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE anthropogenic warming; severe drought events; El Nino; Indian Ocean
   dipole; multimodel analysis; forest fire future projection
ID EL-NINO; INDIAN-OCEAN; FOREST-FIRES; DROUGHT; TEMPERATURE; RAINFALL;
   EVENTS; DIPOLE; REGION; ASIA
AB Uncontrolled biomass burning in Indonesia during drought periods damages the landscape, degrades regional air quality, and acts as a disproportionately large source of greenhouse gas emissions. The expansion of forest fires is mostly observed in October in Sumatra favored by persistent droughts during the dry season from June to November. The contribution of anthropogenic warming to the probability of severe droughts is not yet clear. Here, we show evidence that past events in Sumatra were exacerbated by anthropogenic warming and that they will become more frequent under a future emissions scenario. By conducting two sets of atmospheric general circulation model ensemble experiments driven by observed sea surface temperature for 1960-2011, one with and one without an anthropogenic warming component, we found that a recent weakening of the Walker circulation associated with tropical ocean warming increased the probability of severe droughts in Sumatra, despite increasing tropical-mean precipitation. A future increase in the frequency of droughts is then suggested from our analyses of the Coupled Model Intercomparison Project Phase 5 model ensembles. Increasing precipitation to the north of the equator accompanies drier conditions over Indonesia, amplified by enhanced ocean surface warming in the central equatorial Pacific. The resultant precipitation decrease leads to a similar to 25% increase in severe drought events from 1951-2000 to 2001-2050. Our results therefore indicate the global warming impact to a potential of wide-spreading forest fires over Indonesia, which requires mitigation policy for disaster prevention.
C1 [Lestari, R. Kartika; Watanabe, Masahiro; Kimoto, Masahide] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778568, Japan.
   [Imada, Yukiko] Japan Meteorol Agcy, Meteorol Res Inst, Tsukuba, Ibaraki 3050052, Japan.
   [Shiogama, Hideo] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan.
   [Field, Robert D.] Columbia Univ, Dept Appl Phys & Appl Math, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
   [Takemura, Toshihiko] Kyushu Univ, Appl Mech Res Inst, Fukuoka 8168580, Japan.
RP Lestari, RK (reprint author), Univ Tokyo, Atmosphere & Ocean Res Inst, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778568, Japan.
EM kartika@aori.u-tokyo.ac.jp
RI kimoto, masahide/P-9077-2014; Shiogama, Hideo/B-9598-2012; Takemura,
   Toshihiko/C-2822-2009; Kyushu, RIAM/F-4018-2015; U-ID,
   Kyushu/C-5291-2016
OI Shiogama, Hideo/0000-0001-5476-2148; Takemura,
   Toshihiko/0000-0002-2859-6067; 
FU Program for Risk Information on Climate Change (SOUSEI program) from
   Ministry of Education, Culture, Sports, Science and Technology (MEXT),
   Japan
FX We acknowledge the modelling groups, the Program for Climate Model
   Diagnosis and Intercomparison (PCMDI) and the WCRP's Working Group on
   Coupled Modelling (WGCM) for their efforts in making the CMIP5
   multi-model data set available. The data are available at
   http://cmip-pcmdi.llnl.gov/. The observational data supporting this work
   can be accessed from
   www.ncdc.noaa.gov/data-access/land-basedstation-data/land-based-datasets
   for the visibility data, from
   www.ncdc.noaa.gov/temp-and-precip/ghcn-gridded-products. php for GHCN
   gridded precipitation data, from www.metoffice.gov.uk/hadobs/hadisst/
   for HadISST data, and from
   http://jra.kishou.go.jp/JRA-55/index_en.html#jra-55 for Japan 55-year
   Reanalysis (JRA-55) data. This work was supported by the Program for
   Risk Information on Climate Change (SOUSEI program) from Ministry of
   Education, Culture, Sports, Science and Technology (MEXT), Japan.
NR 31
TC 5
Z9 5
U1 0
U2 12
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 OCT
PY 2014
VL 9
IS 10
AR 104010
DI 10.1088/1748-9326/9/10/104010
PG 7
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AT5DP
UT WOS:000344964000014
ER

PT J
AU Sultana, J
   Bose, B
   Kazanas, D
AF Sultana, Joseph
   Bose, Benjamin
   Kazanas, Demosthenes
TI Neutron star structure in the presence of conformally coupled scalar
   fields
SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D
LA English
DT Article
DE Scalar-tensor theory; scalar field; neutron stars
ID ENERGY-MOMENTUM TENSOR; BOSON-FERMION STARS; GENERAL-RELATIVITY;
   BLACK-HOLES; GRAVITY; MATTER; PRINCIPLE; UNIVERSE; DENSITY; HYPERNUCLEI
AB Neutron star models are studied in the context of scalar-tensor theories of gravity in the presence of a conformally coupled scalar field, using two different numerical equations of state (EoS) representing different degrees of stiffness. In both cases we obtain a complete solution by matching the interior numerical solution of the coupled Einstein-scalar field hydrostatic equations, with an exact metric on the surface of the star. These are then used to find the effect of the scalar field and its coupling to geometry, on the neutron star structure, particularly the maximum neutron star mass and radius. We show that in the presence of a conformally coupled scalar field, neutron stars are less dense and have smaller masses and radii than their counterparts in the minimally coupled case, and the effect increases with the magnitude of the scalar field at the center of the star.
C1 [Sultana, Joseph; Bose, Benjamin] Univ Malta, Fac Sci, Dept Math, MSD-2080 Msida, Malta.
   [Kazanas, Demosthenes] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Sultana, J (reprint author), Univ Malta, Fac Sci, Dept Math, MSD-2080 Msida, Malta.
EM joseph.sultana@um.edu.mt; nebblub@gmail.com; demos.kazanas@nasa.gov
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. We would like to thank the
   anonymous referee for his/her suggestions and for mentioning some useful
   additional references.
NR 74
TC 2
Z9 2
U1 1
U2 4
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE
SN 0218-2718
EI 1793-6594
J9 INT J MOD PHYS D
JI Int. J. Mod. Phys. D
PD OCT
PY 2014
VL 23
IS 11
AR 1450090
DI 10.1142/S0218271814500904
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT5RJ
UT WOS:000344999300007
ER

PT J
AU Dutton, PH
   Jensen, MP
   Frutchey, K
   Frey, A
   LaCasella, E
   Balazs, GH
   Cruce, J
   Tagarino, A
   Farman, R
   Tatarata, M
AF Dutton, Peter H.
   Jensen, Michael P.
   Frutchey, Karen
   Frey, Amy
   LaCasella, Erin
   Balazs, George H.
   Cruce, Jennifer
   Tagarino, Alden
   Farman, Richard
   Tatarata, Miri
TI Genetic Stock Structure of Green Turtle (Chelonia mydas) Nesting
   Populations across the Pacific Islands
SO PACIFIC SCIENCE
LA English
DT Article
ID CONTROL REGION SEQUENCES; MITOCHONDRIAL-DNA; DERMOCHELYS-CORIACEA; MIXED
   STOCKS; PHYLOGEOGRAPHY; ATLANTIC; MTDNA; CONSERVATION; MARKERS
AB More than two decades have passed since the first studies documenting genetic population structure of green turtles (Chelonia mydas) were published. Since then many more have followed and characterization of the genetic structure of green turtle rookeries now covers most of the global distribution of the species, benefitting conservation of this threatened species worldwide. However, important data gaps still exist across a large part of the western and central Pacific Ocean (WCPO). This large area is made up of hundreds of scattered islands and atolls of Micronesia, Melanesia, and Polynesia, most of which are remote and difficult to access. In this study, we assessed stock structure of green turtles throughout the WCPO using mitochondrial (mt) DNA from 805 turtles sampled across 25 nesting locations. We examined whether sequencing longer fragments (770 bp) of the control region increases resolution of stock structure and used genetic analysis to evaluate level of demographic connectivity among island nesting populations in the WCPO. We identified a total of 25 haplotypes characterized by polymorphism within the 770 bp sequences, including five new variants of haplotypes that were indistinguishable with shorter 384 bp reads from previous studies. Stock structure analysis indicated that rookeries separated by more than 1,000 km were significantly differentiated from each other, but neighboring rookeries within 500 km showed no genetic differentiation. Results presented in this paper establish that sequencing of longer fragments (770 bp) of the control region does in some cases increase resolution and that there are at least seven independent stocks in the region.
C1 [Dutton, Peter H.; Jensen, Michael P.; Frey, Amy; LaCasella, Erin] Natl Marine Fisheries Serv, Marine Mammal & Turtle Div, SW Fisheries Sci Ctr, NOAA, La Jolla, CA 92037 USA.
   [Frutchey, Karen] Univ Hawaii Manoa, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA.
   [Balazs, George H.] Natl Marine Fisheries Serv, Marine Turde Res Program, Pacific Isl Fisheries Sci Ctr, NOAA, Honolulu, HI 96818 USA.
   [Cruce, Jennifer] US Fish & Wildlife Serv, Guam Natl Wildlife Refuge, Dededo, GU 96912 USA.
   [Tagarino, Alden] Amer Samoa Govt, Dept Marine & Wildlife Resources, Pago Pago, AS 96799 USA.
   [Farman, Richard] Aquarium Lagon, Grand Terre 98807, New Caledonia.
   [Tatarata, Miri] Direct Environm, Papeete 98713, Fr Polynesia.
RP Dutton, PH (reprint author), Natl Marine Fisheries Serv, Marine Mammal & Turtle Div, SW Fisheries Sci Ctr, NOAA, 8901 La Jolla Shores Dr, La Jolla, CA 92037 USA.
EM Peter.Dutton@noaa.gov
NR 51
TC 10
Z9 10
U1 3
U2 26
PU UNIV HAWAII PRESS
PI HONOLULU
PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA
SN 0030-8870
EI 1534-6188
J9 PAC SCI
JI Pac. Sci.
PD OCT
PY 2014
VL 68
IS 4
BP 451
EP 464
DI 10.2984/68.4.1
PG 14
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA AU0JO
UT WOS:000345309400001
ER

PT J
AU Zanetti, LJ
   Mauk, BH
   Fox, NJ
   Barnes, RJ
   Weiss, M
   Sotirelis, TS
   Raouafi, NE
   Kessel, RL
   Becker, HN
AF Zanetti, L. J.
   Mauk, B. H.
   Fox, N. J.
   Barnes, R. J.
   Weiss, M.
   Sotirelis, T. S.
   Raouafi, N. -E.
   Kessel, R. L.
   Becker, H. N.
TI The Evolving Space Weather System-Van Allen Probes Contribution
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE radiation belts
AB The overarching goal and purpose of the study of space weather is clearto understand and address the issues caused by solar disturbances on humans and technological systems. Space weather has evolved in the past few decades from a collection of concerned agencies and researchers to a critical function of the National Weather Service of NOAA. The general effects have also evolved from the well-known telegraph disruptions of the mid-1800s to modern day disturbances of the electric power grid, communications and navigation, human spaceflight and spacecraft systems. The last two items in this list, and specifically the effects of penetrating radiation, were the impetus for the space weather broadcast implemented on NASA's Van Allen Probes' twin pair of satellites, launched in August of 2012 and orbiting directly through Earth's severe radiation belts. The Van Allen Probes mission, formerly the Radiation Belt Storm Probes (RBSP), was renamed soon after launch to honor the discoverer of Earth's radiation belts at the beginning of the space age, the late James Van Allen (the spacecraft themselves are still referred to as RBSP-A and RBSP-B). The Van Allen Probes are one part of NASA's Living With a Star program formulated to advance the scientific understanding of the connection between solar disturbances, the resulting heliospheric conditions, and their effects on the geospace and Earth environment.
C1 [Zanetti, L. J.; Mauk, B. H.; Fox, N. J.; Barnes, R. J.; Weiss, M.; Sotirelis, T. S.; Raouafi, N. -E.; Kessel, R. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20707 USA.
   [Becker, H. N.] NASA Headquarters, Jet Prop Lab, Washington, DC USA.
RP Zanetti, LJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20707 USA.
EM larry.zanetti@jhuapl.edu
RI Raouafi, Nour/C-2286-2016; Fox, Nicola/P-6692-2016; Mauk,
   Barry/E-8420-2017
OI Raouafi, Nour/0000-0003-2409-3742; Fox, Nicola/0000-0003-3411-4228;
   Mauk, Barry/0000-0001-9789-3797
NR 14
TC 0
Z9 0
U1 2
U2 7
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 OCT
PY 2014
VL 12
IS 10
BP 577
EP 581
DI 10.1002/2014SW001108
PG 5
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences
GA AT9UI
UT WOS:000345271400004
ER

PT J
AU Juusola, L
   Facsko, G
   Honkonen, I
   Janhunen, P
   Vanhamaki, H
   Kauristie, K
   Laitinen, TV
   Milan, SE
   Palmroth, M
   Tanskanen, EI
   Viljanen, A
AF Juusola, L.
   Facsko, G.
   Honkonen, I.
   Janhunen, P.
   Vanhamaeki, H.
   Kauristie, K.
   Laitinen, T. V.
   Milan, S. E.
   Palmroth, M.
   Tanskanen, E. I.
   Viljanen, A.
TI Statistical comparison of seasonal variations in the GUMICS-4 global MHD
   model ionosphere and measurements
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE MHD simulation; high-latitude ionosphere; seasonal variations
ID INTERPLANETARY MAGNETIC-FIELD; ELEMENTARY CURRENT SYSTEMS; SCALE
   BIRKELAND CURRENTS; HIGH-LATITUDE CONVECTION; GEOMAGNETIC-ACTIVITY;
   ELECTRIC-FIELDS; CHAMP SATELLITE; SIMULATIONS; MAGNETOSPHERE;
   CONDUCTIVITY
AB Understanding the capability of a simulation to reproduce observed features is a requirement for its use in operational space weather forecasting. We compare statistically ionospheric seasonal variations in the Grand Unified Magnetosphere-Ionosphere Coupling Simulation (GUMICS-4) global magnetohydrodynamic model with measurements. The GUMICS-4 data consist of a set of runs that was fed with real solar wind measurements and cover the period of 1 year. Ionospheric convection measurements are from the Super Dual Auroral Radar Network (SuperDARN) radars, and electric currents are derived from the magnetic field measured by the CHAMP satellite. Auroral electrojet indices are used to examine the disturbance magnetic field on ground. The signatures of electrodynamic coupling between the magnetosphere and ionosphere extend to lower latitudes in GUMICS-4 than in observations, and key features of the auroral ovalsthe Region 2 field-aligned currents, electrojets, Harang discontinuity, and ring of enhanced conductivityare not properly reproduced. The ground magnetic field is even at best about 5 times weaker than measurements, which can be a problem for forecasting geomagnetically induced currents. According to the measurements, the ionospheric electrostatic potential does not change significantly from winter to summer but field-aligned currents enhance, whereas in GUMICS-4, the electrostatic potential weakens from winter to summer but field-aligned currents do not change. This could be a consequence of the missing Region 2 currents: the Region 1 current has to close with itself across the polar cap, which makes it sensitive to solar UV conductivity. Precipitation energy and conductance peak amplitudes in GUMICS-4 agree with observations.
C1 [Juusola, L.; Facsko, G.; Honkonen, I.; Janhunen, P.; Vanhamaeki, H.; Kauristie, K.; Laitinen, T. V.; Palmroth, M.; Tanskanen, E. I.; Viljanen, A.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
   [Facsko, G.] HAS, Geodet & Geophys Inst, RCAES, Sopron, Hungary.
   [Honkonen, I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Vanhamaeki, H.] Univ Oulu, Dept Phys, FIN-90570 Oulu, Finland.
   [Milan, S. E.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
RP Juusola, L (reprint author), Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
EM Liisa.Juusola@fmi.fi
OI Vanhamaki, Heikki/0000-0002-3454-0350
FU Space Agency of the German Aerospace Center (DLR) through the Federal
   Ministry of Economics and Technology [50EE0944]; European Union [263325,
   260330]; Academy of Finland [137900, 272157]; NASA Postdoc Program; STFC
   grant [ST/K001000/1]; OTKA grant of the Hungarian Scientific Research
   Fund [K75640]
FX We thank P. Ritter for providing the CHAMP data. The CHAMP mission is
   sponsored by the Space Agency of the German Aerospace Center (DLR)
   through funds of the Federal Ministry of Economics and Technology,
   following a decision of the German Federal Parliament (grant code
   50EE0944). The data retrieval and operation of the CHAMP satellite by
   the German Space Operations Center (GSOC) of DLR is acknowledged. We
   acknowledge NASA/GSFC's Space Physics Data Facility's OMNIWeb service
   and OMNI data. The research leading to these results has received
   funding from the European Union Seventh Framework Programme
   (FP7/2007-2013) under grant agreements 263325 (ECLAT) and 260330
   (EURISGIC). The work of L. Juusola was supported by the Academy of
   Finland project 137900, I.Honkonen by the NASA Postdoc Program, S.E.
   Milan by the STFC grant ST/K001000/1, and G. Facsko by the OTKA grant
   K75640 of the Hungarian Scientific Research Fund. We acknowledge the
   financial support by the Academy of Finland to the ReSoLVE Center of
   Excellence (project 272157).
NR 56
TC 6
Z9 6
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD OCT
PY 2014
VL 12
IS 10
BP 582
EP 600
DI 10.1002/2014SW001082
PG 19
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences
GA AT9UI
UT WOS:000345271400005
ER

PT J
AU Nowlan, CR
   Martin, RV
   Philip, S
   Lamsal, LN
   Krotkov, NA
   Marais, EA
   Wang, S
   Zhang, Q
AF Nowlan, C. R.
   Martin, R. V.
   Philip, S.
   Lamsal, L. N.
   Krotkov, N. A.
   Marais, E. A.
   Wang, S.
   Zhang, Q.
TI Global dry deposition of nitrogen dioxide and sulfur dioxide inferred
   from space-based measurements
SO GLOBAL BIOGEOCHEMICAL CYCLES
LA English
DT Article
DE dry deposition; OMI; sulfur dioxide; nitrogen dioxide
ID OZONE MONITORING INSTRUMENT; GENERAL-CIRCULATION MODEL; BIOGENIC NOX
   EMISSIONS; CLEAN-AIR STATUS; UNITED-STATES; REACTIVE NITROGEN;
   BOUNDARY-LAYER; ATMOSPHERIC DEPOSITION; OXIDIZED NITROGEN; TRENDS
   NETWORK
AB A method is developed to estimate global NO2 and SO2 dry deposition fluxes at high spatial resolution (0.1 degrees x0.1 degrees) using satellite measurements from the Ozone Monitoring Instrument (OMI) on the Aura satellite, in combination with simulations from the Goddard Earth Observing System chemical transport model (GEOS-Chem). These global maps for 2005-2007 provide a data set for use in examining global and regional budgets of deposition. In order to properly assess SO2 on a global scale, a method is developed to account for the geospatial character of background offsets in retrieved satellite columns. Globally, annual dry deposition to land estimated from OMI as NO2 contributes 1.5 0.5Tg of nitrogen and as SO2 contributes 13.7 4.0Tg of sulfur. Differences between OMI-inferred NO2 dry deposition fluxes and those of other models and observations vary from excellent agreement to an order of magnitude difference, with OMI typically on the low end of estimates. SO2 dry deposition fluxes compare well with in situ Clear Air Status and Trends Network-inferred flux over North America (slope=0.98, r=0.71). The most significant NO2 dry deposition flux to land per area occurs in the Pearl River Delta, China, at 13.9 kg N ha(-1) yr(-1), while SO2 dry deposition has a global maximum rate of 72.0 kg S ha(-1) yr(-1) to the east of Jinan in China's Shandong province. Dry deposition fluxes are explored in several urban areas, where NO2 contributes on average 9-36% and as much as 85% of total NOy dry deposition.
C1 [Nowlan, C. R.; Martin, R. V.; Philip, S.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
   [Nowlan, C. R.; Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
   [Lamsal, L. N.; Krotkov, N. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Marais, E. A.] Harvard Univ, Cambridge, MA 02138 USA.
   [Wang, S.] Tsinghua Univ, Sch Environm, Beijing 100084, Peoples R China.
   [Zhang, Q.] Tsinghua Univ, Ctr Earth Syst Sci, Beijing 100084, Peoples R China.
RP Nowlan, CR (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
EM cnowlan@cfa.harvard.edu
RI Zhang, Qiang/D-9034-2012; Martin, Randall/C-1205-2014; Krotkov,
   Nickolay/E-1541-2012; 
OI Martin, Randall/0000-0003-2632-8402; Krotkov,
   Nickolay/0000-0001-6170-6750; Nowlan, Caroline/0000-0002-8718-9752;
   Marais, Eloise/0000-0001-5477-8051
FU Environment Canada; Natural Sciences and Engineering Research Council of
   Canada (NSERC)
FX This work was supported by Environment Canada and the Natural Sciences
   and Engineering Research Council of Canada (NSERC). We thank Robert Vet
   for helpful comments during the early stages of this project, Aaron van
   Donkelaar and Shailesh Kharol for code, Daniel Jacob for comments on
   urban deposition, and Laurens Ganzeveld for helpful comments on the
   manuscript. MODIS LAI data were obtained through the NASA Land Processes
   Distributed Active Archive Center (LP DAAC) USGS/Earth Resources
   Observation and Science (EROS) Center. Global dry deposition data from
   this study are available from the authors by request to
   cnowlan@cfa.harvard.edu.
NR 102
TC 8
Z9 8
U1 2
U2 37
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0886-6236
EI 1944-9224
J9 GLOBAL BIOGEOCHEM CY
JI Glob. Biogeochem. Cycle
PD OCT
PY 2014
VL 28
IS 10
BP 1025
EP 1043
DI 10.1002/2014GB004805
PG 19
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
   Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
   Sciences
GA AT2XK
UT WOS:000344797500002
ER

PT J
AU Teverovsky, A
AF Teverovsky, Alexander
TI Absorption Voltages and Insulation Resistance in Ceramic Capacitors with
   Cracks
SO IEEE TRANSACTIONS ON DIELECTRICS AND ELECTRICAL INSULATION
LA English
DT Article
DE Ceramic capacitor; insulation resistance; dielectric absorption;
   cracking
ID DIELECTRIC ABSORPTION
AB Time dependence of absorption voltages (V-abs) in different types of low-voltage X5R and X7R ceramic capacitors was monitored for a maximum duration of hundred hours after polarization. To evaluate the effect of mechanical defects on V-abs, cracks in the dielectric were introduced either mechanically or by thermal shock. The maximum absorption voltage, time to roll-off, and the rate of voltage decrease are shown to depend on the crack-related leakage currents and insulation resistance in the parts. A simple model that is based on the Dow equivalent circuit for capacitors with absorption has been developed to assess the insulation resistance of capacitors. Standard measurements of the insulation resistance, contrary to the measurements based on V-abs, are not sensitive to the presence of mechanical defects and fail to reveal capacitors with cracks.
C1 NASA GSFC, ASRC Space & Def, Greenbelt, MD 20771 USA.
RP Teverovsky, A (reprint author), NASA GSFC, ASRC Space & Def, Code 562,B-22,Rm C163, Greenbelt, MD 20771 USA.
FU NASA Electronic Parts and Packaging (NEPP) program
FX This work was sponsored by the NASA Electronic Parts and Packaging
   (NEPP) program. The author is thankful to Michael Sampson, NEPP Program
   Manager, for support of this investigation, and to Jaemi Herzberger
   (UMCP) for assistance with preparing the manuscript.
NR 16
TC 0
Z9 0
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1070-9878
EI 1558-4135
J9 IEEE T DIELECT EL IN
JI IEEE Trns. Dielectr. Electr. Insul.
PD OCT
PY 2014
VL 21
IS 5
BP 2020
EP 2027
DI 10.1109/TDEI.2014.004082
PG 8
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA AS9XC
UT WOS:000344590800003
ER

PT J
AU Howard, DC
   Saha, PK
   Shankar, S
   England, TD
   Cardoso, AS
   Diestelhorst, RM
   Jung, S
   Cressler, JD
AF Howard, Duane C.
   Saha, Prabir K.
   Shankar, Subramaniam
   England, Troy D.
   Cardoso, Adilson S.
   Diestelhorst, Ryan M.
   Jung, Seungwoo
   Cressler, John D.
TI A SiGe 8-18-GHz Receiver With Built-In-Testing Capability for
   Self-Healing Applications
SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES
LA English
DT Article
DE Built-in test (BIT); built-in self-test (BIST); SiGe BiCMOS; microwave
   integrated circuits (ICs); signal generation; tunable microwave circuits
ID CIRCUITS; AMPLIFIER
AB A wideband (8-18 GHz) built-in test receiver in silicon-germanium technology is presented. The receiver chain consists of a low-noise amplifier (LNA), an image-reject mixer, on-chip automatic gain control ring oscillator sources that are used to provide test signals of a predefined amplitude, and control circuitry in the form of digital-to-analog converters and data registers. Both the LNA and the mixer circuit blocks incorporate tuning knobs to enable tuning of RF metrics to ensure consistent performance and mitigate the negative effects of process, voltage, and temperature variations, aging, and damage from extreme environments such as ionizing radiation. A maximum post-healed gain greater than 30 dB, an image rejection ratio exceeding 30 dB, output third-order intercept point greater than 8 dBm, and noise figure less than 9 dB are obtained in measurement. An automated healing algorithm was developed and shown to be effective at improving the overall performance of the receiver. The receiver was fabricated in an 0.18-mu m SiGe BiCMOS process with a peak f(T) of 150 GHz, and consumes 240-260 mA from a 4-V supply.
C1 [Howard, Duane C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Saha, Prabir K.; Cardoso, Adilson S.; Jung, Seungwoo; Cressler, John D.] Georgia Inst Technol, Dept Elect & Comp Engn, Atlanta, GA 30332 USA.
   [Shankar, Subramaniam] Inphi Corp, Thousand Oaks, CA 91362 USA.
   [England, Troy D.] Sandia Natl Labs, Albuquerque, NM 87123 USA.
   [Diestelhorst, Ryan M.] NextInput Inc, Atlanta, GA 30308 USA.
RP Howard, DC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM duane.c.howard@jpl.nasa.gov
FU Defense Advanced Research Projects Agency (DARPA) under HEALICs Program
FX This work was supported by the Defense Advanced Research Projects Agency
   (DARPA) under the HEALICs Program.
NR 21
TC 5
Z9 5
U1 0
U2 2
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 OCT
PY 2014
VL 62
IS 10
BP 2370
EP 2380
DI 10.1109/TMTT.2014.2345334
PG 11
WC Engineering, Electrical & Electronic
SC Engineering
GA AT5NX
UT WOS:000344990600015
ER

PT J
AU Wong, TH
   Yu, JR
   Bai, YX
   Johnson, W
   Chen, SS
   Petros, M
   Singh, UN
AF Wong, Teh-Hwa
   Yu, Jirong
   Bai, Yingxin
   Johnson, William
   Chen, Songsheng
   Petros, Mulugeta
   Singh, Upendra N.
TI Sensitive infrared signal detection by upconversion technique
SO OPTICAL ENGINEERING
LA English
DT Article
DE Nonlinear; sum frequency generation; periodically poled lithium niobate;
   2.05 mu m; single-photon counting module
ID POLED LITHIUM-NIOBATE; MU-M; LINBO3; GENERATION
AB We demonstrated upconversion assisted detection of a 2.05-mu m signal by sum frequency generation to generate a 700-nm light using a bulk periodically poled lithium niobate crystal. The achieved 94% intrinsic upconversion efficiency and 22.58% overall detection efficiency at a pW level of 2.05 mu m pave the path to detect extremely weak infrared (IR) signals for remote sensing applications. (C) Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License.
C1 [Wong, Teh-Hwa; Bai, Yingxin] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
   [Yu, Jirong; Chen, Songsheng; Petros, Mulugeta; Singh, Upendra N.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Johnson, William] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
RP Wong, TH (reprint author), Sci Syst & Applicat Inc, One Enterprise Pkwy,Suite 300, Hampton, VA 23666 USA.
EM teh-hwa.wong@ssaihq.com
FU NASA LaRC IRAD Program
FX This work was supported by NASA LaRC IRAD Program.
NR 16
TC 1
Z9 1
U1 2
U2 8
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
J9 OPT ENG
JI Opt. Eng.
PD OCT
PY 2014
VL 53
IS 10
AR 107102
DI 10.1117/1.OE.53.10.107102
PG 6
WC Optics
SC Optics
GA AT4AG
UT WOS:000344878300037
ER

PT J
AU Bessho, N
   Bhattacharjee, A
AF Bessho, N.
   Bhattacharjee, A.
TI Instability of the current sheet in the Earth's magnetotail with normal
   magnetic field
SO PHYSICS OF PLASMAS
LA English
DT Article
ID 2-DIMENSIONAL MAGNETOTAIL; COLLISIONLESS RECONNECTION; TEARING
   STABILITY; EQUILIBRIA; DYNAMICS; ONSET; TAIL
AB Instability of a current sheet in the Earth's magnetotail has been investigated by two-dimensional fully kinetic simulations. Two types of magnetic configuration have been studied; those with uniform normal magnetic field along the current sheet and those in which the normal magnetic field has a spatial hump. The latter configuration has been proposed by Sitnov and Schindler [Geophys. Res. Lett. 37, L08102 (2010)] as one in which ion tearing modes might grow. The first type of configuration exhibits electron tearing modes when the normal magnetic field is small. The second type of configuration exhibits an instability which does not tear or change the topology of magnetic field lines. The hump in the initial configuration can propagate Earthward in the nonlinear regime, leading to the formation of a dipolarization front. Secondary magnetic islands can form in regions where the normal magnetic field is very weak. Under no conditions do we find the ion tearing instability. (C) 2014 AIP Publishing LLC.
C1 [Bessho, N.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Bessho, N.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
   [Bhattacharjee, A.] Princeton Univ, Dept Astrophys Sci, Ctr Heliophys, Princeton, NJ 08543 USA.
   [Bhattacharjee, A.] Princeton Univ, Princeton Plasma Phys Lab, Princeton, NJ 08543 USA.
RP Bessho, N (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM naoki.bessho@nasa.gov
FU NSF [ATM-090315, AGS-1338944]; NASA [NNX09AJ86G]; DOE under Center for
   Integrated Computation and Analysis of Reconnection and Turbulence
   [DE-FG02-14-07ER46372]
FX It is a pleasure to acknowledge trenchant discussions with Dr. M. Sitnov
   on the subject of ion tearing modes, and we thank him for his
   encouragement to continue with our research on this problem. This work
   was supported by NSF Grant Nos. ATM-090315 and AGS-1338944, NASA Grant
   No. NNX09AJ86G, and DOE Grant No. DE-FG02-14-07ER46372, under the
   auspices of the Center for Integrated Computation and Analysis of
   Reconnection and Turbulence. We acknowledge the use of computer
   resources at the National Energy Research Scientific Computing Center.
NR 21
TC 9
Z9 9
U1 0
U2 3
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 OCT
PY 2014
VL 21
IS 10
AR 102905
DI 10.1063/1.4899043
PG 6
WC Physics, Fluids & Plasmas
SC Physics
GA AS9YG
UT WOS:000344593700067
ER

PT J
AU Conroy, KE
   Prsa, A
   Stassun, KG
   Bloemen, S
   Parvizi, M
   Quarles, B
   Boyajian, T
   Barclay, T
   Shporer, A
   Latham, DW
   Abdul-Masih, M
AF Conroy, Kyle E.
   Prsa, Andrej
   Stassun, Keivan G.
   Bloemen, Steven
   Parvizi, Mahmoud
   Quarles, Billy
   Boyajian, Tabetha
   Barclay, Thomas
   Shporer, Avi
   Latham, David W.
   Abdul-Masih, Michael
TI Kepler Eclipsing Binary Stars. V. Identification of 31 Candidate
   Eclipsing Binaries in the K2 Engineering Dataset
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID DATA RELEASE; PLANET; I.
AB Over 2500 eclipsing binaries were identified and characterized from the ultraprecise photometric data provided by the Kepler space telescope. Kepler is now beginning its second mission, K2, which is proving to again provide ultraprecise photometry for a large sample of eclipsing binary stars. In the 1951 light curves covering 12 days in the K2 engineering dataset, we have identified and determined the ephemerides for 31 candidate eclipsing binaries that demonstrate the capabilities for eclipsing binary science in the upcoming campaigns in K2. Of those, 20 are new discoveries. We describe both manual and automated approaches to harvesting the complete set of eclipsing binaries in the K2 data, provide identifications and details for the full set of candidate eclipsing binaries present in the engineering dataset, and discuss the prospects for application of eclipsing binary searches in the K2 mission.
C1 [Conroy, Kyle E.; Stassun, Keivan G.; Parvizi, Mahmoud] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
   [Prsa, Andrej; Abdul-Masih, Michael] Villanova Univ, Dept Astrophys & Planetary Sci, Villanova, PA 19085 USA.
   [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
   [Bloemen, Steven] Radboud Univ Nijmegen, Dept Astrophys, Inst Math Astrophys & Particle Phys, NL-6500 GL Nijmegen, Netherlands.
   [Bloemen, Steven] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium.
   [Quarles, Billy; Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Boyajian, Tabetha] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
   [Barclay, Thomas] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
   [Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
   [Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Conroy, KE (reprint author), Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
OI Boyajian, Tabetha/0000-0001-9879-9313
FU NASA Astrophysical Data Analysis Program [NNX12AE22G]; NASA Kepler
   Participating Scientist Program [NNX12AD20G]; Foundation for Fundamental
   Research on Matter (FOM), which is part of the Netherlands Organisation
   for Scientific Research (NWO)
FX The authors gratefully acknowledge everybody who has made Kepler, and
   especially the K2 mission, possible. K. E. C. and K. G. S. gratefully
   acknowledge support from NASA Astrophysical Data Analysis Program grant
   NNX12AE22G. A. P. gratefully acknowledges support from the NASA Kepler
   Participating Scientist Program grant NNX12AD20G. S. B. is supported by
   the Foundation for Fundamental Research on Matter (FOM), which is part
   of the Netherlands Organisation for Scientific Research (NWO). This
   research has made use of the SIMBAD database, operated at CDS,
   Strasbourg, France.
NR 16
TC 6
Z9 6
U1 0
U2 2
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 OCT
PY 2014
VL 126
IS 944
BP 914
EP 922
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT1WD
UT WOS:000344720900003
ER

PT J
AU Al-Hamdan, M
   Cruise, J
   Rickman, D
   Quattrochi, D
AF Al-Hamdan, Mohammad
   Cruise, James
   Rickman, Douglas
   Quattrochi, Dale
TI Forest Stand Size-Species Models Using Spatial Analyses of Remotely
   Sensed Data
SO REMOTE SENSING
LA English
DT Article
DE remote sensing; fractal dimensions; Moran's I; forested landscapes;
   size-species models
ID SENSING DATA; BOREAL FOREST; ABOVEGROUND BIOMASS; TEMPERATE FOREST; STEM
   VOLUME; LANDSAT TM; SAR DATA; LIDAR; INVENTORY; RADAR
AB Regression models to predict stand size classes (sawtimber and saplings) and categories of species (hardwood and softwood) from fractal dimensions (FD) and Moran's I derived from Landsat Thematic Mapper (TM) data were developed. Three study areas (Oakmulgee National Forest, Bankhead National Forest, and Talladega National Forest) were randomly selected and used to develop the prediction models, while one study area, Chattahoochee National Forest, was saved for validation. This study has shown that these spatial analytical indices (FD and Moran's I) can distinguish between different forest trunk size classes and different categories of species (hardwood and softwood) using Landsat TM data. The results of this study also revealed that there is a linear relationship between each one of the spatial indices and the percentages of sawtimber-saplings size classes and hardwood-softwood categories of species. Given the high number of factors causing errors in the remotely sensed data as well as the Forest Inventory Analysis (FIA) data sets and compared to other studies in the research literature, the sawtimber-saplings models and hardwood-softwood models were reasonable in terms of significance and the levels of explained variance for both spatial indices FD and Moran's I. The mean absolute percentage errors associated with the stand size classes prediction models and categories of species prediction models that take topographical elevation into consideration ranged from 4.4% to 19.8% and from 12.1% to 18.9%, respectively, while the root mean square errors ranged from 10% to 14% and from 11% to 13%, respectively.
C1 [Al-Hamdan, Mohammad] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Natl Space Sci & Technol Ctr,Global Hydrol & Clim, Huntsville, AL 35805 USA.
   [Cruise, James] Univ Alabama, Ctr Earth Syst Sci, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
   [Rickman, Douglas; Quattrochi, Dale] NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Global Hydrol & Climate Ctr,Earth Sci Off, Huntsville, AL 35805 USA.
RP Al-Hamdan, M (reprint author), NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Natl Space Sci & Technol Ctr,Global Hydrol & Clim, Huntsville, AL 35805 USA.
EM mohammad.alhamdan@nasa.gov; james.cruise@nsstc.uah.edu;
   douglas.l.rickman@nasa.gov; dale.quattrochi@nasa.gov
OI Rickman, Doug/0000-0003-3409-2882
FU U.S. Department of Transportation
FX This project was supported by a grant from the U.S. Department of
   Transportation "Applications of remote sensing and related spatial
   technologies to environmental assessments in transportation." The
   assistance of the project manager, Roger King of Mississippi State
   University, and the USDOT program director, K. Thirumalai is gratefully
   acknowledged. The authors would also like to thank Nina Lam of Louisiana
   State University and Charles Emerson of Western Michigan University for
   their assistance.
NR 67
TC 1
Z9 1
U1 3
U2 14
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD OCT
PY 2014
VL 6
IS 10
BP 9802
EP 9828
DI 10.3390/rs6109802
PG 27
WC Remote Sensing
SC Remote Sensing
GA AS7TQ
UT WOS:000344458000030
ER

PT J
AU Montesano, PM
   Sun, GQ
   Dubayah, R
   Ranson, KJ
AF Montesano, Paul M.
   Sun, Guoqing
   Dubayah, Ralph
   Ranson, Kenneth J.
TI The Uncertainty of Plot-Scale Forest Height Estimates from Complementary
   Spaceborne Observations in the Taiga-Tundra Ecotone
SO REMOTE SENSING
LA English
DT Article
DE ecotone; taiga; tundra; spaceborne; uncertainty; vegetation; structure;
   LiDAR; stereo; photogrammetry
ID GROWING STOCK VOLUME; REMOTE-SENSING DATA; AIRBORNE LIDAR; CANOPY
   HEIGHT; TREE COVER; GEOPOSITIONING ACCURACY; RADAR BACKSCATTER; LARCH
   FORESTS; BIOMASS; IMAGERY
AB Satellite-based estimates of vegetation structure capture broad-scale vegetation characteristics as well as differences in vegetation structure at plot-scales. Active remote sensing from laser altimetry and radar systems is regularly used to measure vegetation height and infer vegetation structural attributes, however, the current uncertainty of their spaceborne measurements is likely to mask actual plot-scale differences in vertical structures in sparse forests. In the taiga (boreal forest)-tundra ecotone (TTE) the accumulated effect of subtle plot-scale differences in vegetation height across broad-scales may be significant. This paper examines the uncertainty of plot-scale forest canopy height measurements in northern Siberia Larix stands by combining complementary canopy surface elevations derived from satellite photogrammetry and ground elevations derived from the Geosciences Laser Altimeter System (GLAS) from the ICESat-1 satellite. With a linear model, spaceborne-derived canopy height measurements at the plot-scale predicted TTE stand height similar to 5 m-similar to 10 m tall (R-2 = 0.55, bootstrapped 95% confidence interval of R-2 = 0.36-0.74) with an uncertainty ranging from +/- 0.86 m-1.37 m. A larger sample may mitigate the broad uncertainty of the model fit, however, the methodology provides a means for capturing plot-scale canopy height and its uncertainty from spaceborne data at GLAS footprints in sparse TTE forests and may serve as a basis for scaling up plot-level TTE vegetation height measurements to forest patches.
C1 [Montesano, Paul M.; Sun, Guoqing; Ranson, Kenneth J.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
   [Montesano, Paul M.; Sun, Guoqing; Dubayah, Ralph] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
   [Montesano, Paul M.] Sigma Space Corp, Lanham, MD 20706 USA.
RP Montesano, PM (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
EM paul.m.montesano@nasa.gov; guoqing.sun@nasa.gov; dubayah@umd.edu;
   jon.ranson@nasa.gov
RI Ranson, Kenneth/G-2446-2012
OI Ranson, Kenneth/0000-0003-3806-7270
FU NASA's Terrestrial Ecology Program; NASA's Ames Stereo Pipeline software
FX This work was supported by NASA's Terrestrial Ecology Program and was
   made possible in part through field expedition contributions from Ross
   Nelson, Viacheslav Kharuk, Sergey Im, Pavel Oskorbin, and Muhktar
   Naurzbaev. We acknowledge the work of Oleg Alexandrov and Zachary
   Moratto for development and on-going support of NASA's Ames Stereo
   Pipeline software. We thank the 5 anonymous reviewers for helping to
   significantly improve this manuscript.
NR 78
TC 7
Z9 7
U1 5
U2 21
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD OCT
PY 2014
VL 6
IS 10
BP 10070
EP 10088
DI 10.3390/rs61010070
PG 19
WC Remote Sensing
SC Remote Sensing
GA AS7TQ
UT WOS:000344458000041
ER

PT J
AU Barsi, JA
   Lee, K
   Kvaran, G
   Markham, BL
   Pedelty, JA
AF Barsi, Julia A.
   Lee, Kenton
   Kvaran, Geir
   Markham, Brian L.
   Pedelty, Jeffrey A.
TI The Spectral Response of the Landsat-8 Operational Land Imager
SO REMOTE SENSING
LA English
DT Article
DE Landsat-8; OLI; spectral response; RSR; characterization
AB This paper discusses the pre-launch spectral characterization of the Operational Land Imager (OLI) at the component, assembly and instrument levels and relates results of those measurements to artifacts observed in the on-orbit imagery. It concludes that the types of artifacts observed and their magnitudes are consistent with the results of the pre-launch characterizations. The OLI in-band response was characterized both at the integrated instrument level for a sampling of detectors and by an analytical stack-up of component measurements. The out-of-band response was characterized using a combination of Focal Plane Module (FPM) level measurements and optical component level measurements due to better sensitivity. One of the challenges of a pushbroom design is to match the spectral responses for all detectors so that images can be flat-fielded regardless of the spectral nature of the targets in the imagery. Spectral variability can induce striping (detector-to-detector variation), banding (FPM-to-FPM variation) and other artifacts in the final data products. Analyses of the measured spectral response showed that the maximum discontinuity between FPMs due to spectral filter differences is 0.35% for selected targets for all bands except for Cirrus, where there is almost no signal. The average discontinuity between FPMs is 0.12% for the same targets. These results were expected and are in accordance with the OLI requirements. Pre-launch testing identified low levels (within requirements) of spectral crosstalk amongst the three HgCdTe (Cirrus, SWIR1 and SWIR2) bands of the OLI and on-orbit data confirms this crosstalk in the imagery. Further post-launch analyses and simulations revealed that the strongest crosstalk effect is from the SWIR1 band to the Cirrus band; about 0.2% of SWIR1 signal leaks into the Cirrus. Though the total crosstalk signal is only a few counts, it is evident in some scenes when the in-band cirrus signal is very weak. In moist cirrus-free atmospheres and over typical land surfaces, at least 30% of the cirrus signal was due to the SWIR1 band. In the SWIR1 and SWIR2 bands, crosstalk accounts for no more than 0.15% of the total signal.
C1 [Barsi, Julia A.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA.
   [Lee, Kenton; Kvaran, Geir] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA.
   [Markham, Brian L.; Pedelty, Jeffrey A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Barsi, JA (reprint author), NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Code 618, Greenbelt, MD 20771 USA.
EM julia.barsi@nasa.gov; klee@ball.com; gkvaran@ball.com;
   brian.l.markham@nasa.gov; jeffrey.a.pedelty@nasa.gov
FU NASA [NNG09HP18C, NNG07HW18C]
FX Science Systems and Applications, Inc. work was performed under NASA
   contract NNG09HP18C. Ball Aerospace and Technologies, Corp. was under
   NASA contract NNG07HW18C.
NR 5
TC 19
Z9 19
U1 0
U2 6
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD OCT
PY 2014
VL 6
IS 10
BP 10232
EP 10251
DI 10.3390/rs61010232
PG 20
WC Remote Sensing
SC Remote Sensing
GA AS7TQ
UT WOS:000344458000049
ER

PT J
AU Benafan, O
   Padula, SA
   Skorpenske, HD
   An, K
   Vaidyanathan, R
AF Benafan, O.
   Padula, S. A., II
   Skorpenske, H. D.
   An, K.
   Vaidyanathan, R.
TI Design and implementation of a multiaxial loading capability during
   heating on an engineering neutron diffractometer
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID SHAPE-MEMORY ALLOY; SUPERELASTIC NITI; ELASTIC STRAINS; HIGH-PRESSURE;
   DIFFRACTION; TEXTURE; EVOLUTION; BEHAVIOR; VULCAN; STRESS
AB A gripping capability was designed, implemented, and tested for in situ neutron diffraction measurements during multiaxial loading and heating on the VULCAN engineering materials diffractometer at the spallation neutron source at Oak Ridge National Laboratory. The proposed capability allowed for the acquisition of neutron spectra during tension, compression, torsion, and/or complex loading paths at elevated temperatures. The design consisted of age-hardened, Inconel (R) R 718 grips with direct attachment to the existing MTS load frame having axial and torsional capacities of 100 kN and 400 N m, respectively. Internal cooling passages were incorporated into the gripping system for fast cooling rates during high temperature experiments up to similar to 1000 K. The specimen mounting couplers combined a threaded and hexed end-connection for ease of sample installation/removal without introducing any unwanted loads. Instrumentation of this capability is documented in this work along with various performance parameters. The gripping system was utilized to investigate deformation in NiTi shape memory alloys under various loading/control modes (e.g., isothermal, isobaric, and cyclic), and preliminary results are presented. The measurements facilitated the quantification of the texture, internal strain, and phase fraction evolution in NiTi shape memory alloys under various loading/control modes. (C) 2014 AIP Publishing LLC.
C1 [Benafan, O.; Padula, S. A., II] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
   [Benafan, O.; Vaidyanathan, R.] Univ Cent Florida, Mat Sci & Engn Dept, Adv Mat Proc & Anal Ctr, Orlando, FL 32816 USA.
   [Skorpenske, H. D.; An, K.] Oak Ridge Natl Lab, Spallat Neutron Source, Oak Ridge, TN 37831 USA.
RP Benafan, O (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
EM othmane.benafan@nasa.gov
RI An, Ke/G-5226-2011
OI An, Ke/0000-0002-6093-429X
FU Division of Scientific User Facilities, Office of Basic Energy Sciences,
   U.S. Department of Energy [DE-AC05-00OR22725]; UT-Battelle, LLC.; ORNL
   User Partnership Program for Sample Environment Equipment Development,
   NASA [NNX08AB51A, NNX11AI57A]; NASA Fundamental Aeronautics Program
FX This work has benefited from the use of the Spallation Neutron Source at
   Oak Ridge National Laboratory, which is funded by the Division of
   Scientific User Facilities, Office of Basic Energy Sciences, U.S.
   Department of Energy under Contract No. DE-AC05-00OR22725 with
   UT-Battelle, LLC. Financial support from the ORNL User Partnership
   Program for Sample Environment Equipment Development, NASA (Grants
   NNX08AB51A and NNX11AI57A to UCF) and NASA Fundamental Aeronautics
   Program is gratefully acknowledged. The authors thank D. E. Nicholson
   (University of Central Florida), D. P. Armitage (ORNL), and D. Leech
   (Leech Industries, Inc.) for technical support and experimental
   assistance.
NR 33
TC 2
Z9 2
U1 5
U2 14
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0034-6748
EI 1089-7623
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD OCT
PY 2014
VL 85
IS 10
AR 103901
DI 10.1063/1.4896042
PG 12
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA AS9YL
UT WOS:000344594200045
PM 25362410
ER

PT J
AU Ertel, S
   Absil, O
   Defrere, D
   Le Bouquin, JB
   Augereau, JC
   Marion, L
   Blind, N
   Bonsor, A
   Bryden, G
   Lebreton, J
   Milli, J
AF Ertel, S.
   Absil, O.
   Defrere, D.
   Le Bouquin, J-B.
   Augereau, J-C.
   Marion, L.
   Blind, N.
   Bonsor, A.
   Bryden, G.
   Lebreton, J.
   Milli, J.
TI A near-infrared interferometric survey of debris-disk stars IV. An
   unbiased sample of 92 southern stars observed in H band with
   VLTI/PIONIER
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: interferometric; circumstellar matter; planetary systems;
   zodiacal dust
ID MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; PICTORIS MOVING GROUP; SUN-LIKE
   STARS; AGE-METALLICITY RELATION; GENEVA-COPENHAGEN SURVEY; ALL-SKY
   SURVEY; A-F STARS; HOT DUST; BETA-PICTORIS
AB Context. Detecting and characterizing circumstellar dust is a way to study the architecture and evolution of planetary systems. Cold dust in debris disks only traces the outer regions. Warm and hot exozodiacal dust needs to be studied in order to trace regions close to the habitable zone.
   Aims. We aim to determine the prevalence and to constrain the properties of hot exozodiacal dust around nearby main-sequence stars.
   Methods. We searched a magnitude-limited (H <= 5) sample of 92 stars for bright exozodiacal dust using our VLTI visitor instrument PIONIER in the H band. We derived statistics of the detection rate with respect to parameters, such as the stellar spectral type and age or the presence of a debris disk in the outer regions of the systems. We derived more robust statistics by combining our sample with the results from our CHARA/FLUOR survey in the K band. In addition, our spectrally dispersed data allowed us to put constraints on the emission mechanism and the dust properties in the detected systems.
   Results. We find an overall detection rate of bright exozodiacal dust in the H band of 11% (9 out of 85 targets) and three tentative detections. The detection rate decreases from early type to late type stars and increases with the age of the host star. We do not confirm the tentative correlation between the presence of cold and hot dust found in our earlier analysis of the FLUOR sample alone. Our spectrally dispersed data suggest that either the dust is extremely hot or the emission is dominated by the scattered light in most cases. The implications of our results for the target selection of future terrestrial planet-finding missions using direct imaging are discussed.
C1 [Ertel, S.; Le Bouquin, J-B.; Augereau, J-C.; Milli, J.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
   [Ertel, S.; Le Bouquin, J-B.; Augereau, J-C.; Milli, J.] CNRS, IPAG, F-38000 Grenoble, France.
   [Ertel, S.; Milli, J.] European So Observ, Santiago 19, Chile.
   [Absil, O.; Marion, L.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege, Belgium.
   [Defrere, D.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
   [Blind, N.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
   [Bonsor, A.] Univ Bristol, Sch Phys, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
   [Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Lebreton, J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
   [Lebreton, J.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Ertel, S (reprint author), Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
EM sertel@eso.org
FU French National Research Agency (ANR, EXOZODI) [ANR-2010 BLAN-0505-01];
   PNP-CNES; Universite Joseph Fourier (UJF); Institut de Planetologie et
   d'Astrophysique de Grenoble (IPAG); Agence Nationale pour la Recherche
   [ANR-06-BLAN-0421, ANR-10-BLAN-0505]; Institut National des Science de
   l'Univers (INSU PNP); Institut National des Science de l'Univers (INSU
   PNPS); IPAG; CEA-LETI based on CNES
FX We thank P. Thebault for his indispensable contribution to the EXOZODI
   project. S. Ertel, J.-C. Augereau, and A. Bonsor thank the French
   National Research Agency (ANR, contract ANR-2010 BLAN-0505-01, EXOZODI)
   and PNP-CNES for financial support. PIONIER is funded by the Universite
   Joseph Fourier (UJF), the Institut de Planetologie et d'Astrophysique de
   Grenoble (IPAG), the Agence Nationale pour la Recherche
   (ANR-06-BLAN-0421 and ANR-10-BLAN-0505), and the Institut National des
   Science de l'Univers (INSU PNP and PNPS). The integrated optics beam
   combiner is the result of a collaboration between IPAG and CEA-LETI
   based on CNES R&T funding. The authors warmly thank everyone involved in
   the VLTI project. This work is based on observations made with the ESO
   telescopes. It made use of the Smithsonian/NASA Astrophysics Data System
   (ADS) and of the Centre de Donnees astronomiques de Strasbourg (CDS,
   A&AS 143, 23).
NR 164
TC 20
Z9 20
U1 1
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
   FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2014
VL 570
AR A128
DI 10.1051/0004-6361/201424438
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS3EE
UT WOS:000344158500115
ER

PT J
AU Pineda, JL
   Langer, WD
   Goldsmith, PF
AF Pineda, J. L.
   Langer, W. D.
   Goldsmith, P. F.
TI A Herschel [C II] Galactic plane survey III. [C II] as a tracer of star
   formation
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: star formation; galaxies: ISM; galaxies: evolution
ID 158 MU-M; SPACE-OBSERVATORY MEASUREMENTS; RESOLUTION SPECTRAL TEMPLATES;
   MICROWAVE-ANISOTROPY-PROBE; NEARBY DISK GALAXIES; MILKY-WAY; MOLECULAR
   GAS; INTERSTELLAR-MEDIUM; FORMATION RATES; FORMATION LAW
AB Context. The [C II] 158 mu m line is the brightest far-infrared cooling line in galaxies, representing 0.1 to 1% of their far-infrared continuum emission, and is therefore a potentially powerful tracer of star formation activity. The [C II] line traces different phases of the interstellar medium (ISM), including the diffuse ionized medium, warm and cold atomic clouds, clouds in transition from atomic to molecular, and dense and warm photon dominated regions (PDRs). Therefore without being able to separate the contributions to the [C II] emission, the relationship of this fine structure line emission to star formation has been unclear.
   Aims. We study the relationship between the [C II] emission and the star formation rate (SFR) in the Galactic plane and separate the relationship of different ISM phases to the SFR. We compare these relationships to those in external galaxies and local clouds, allowing examinations of these relationships over a wide range of physical scales.
   Methods. We compare the distribution of the [C II] emission, with its different contributing ISM phases, as a function of Galactocentric distance with the SFR derived from radio continuum observations. We also compare the SFR with the surface density distribution of atomic and molecular gas, including the CO-dark H-2 component.
   Results. The [C II] and SFR are well correlated at Galactic scales with a relationship that is in general agreement with that found for external galaxies. By combining [C II] and SFR data points in the Galactic plane with those in external galaxies and nearby star forming regions, we find that a single scaling relationship between the [C II] luminosity and SFR applies over six orders of magnitude. The [C II] emission from different ISM phases are each correlated with the SFR, but only the combined emission shows a slope that is consistent with extragalactic observations. These ISM components have roughly comparable contributions to the Galactic [C II] luminosity: dense PDRs (30%), cold H I (25%), CO-dark H-2 (25%), and ionized gas (20%). The SFR-gas surface density relationship shows a steeper slope compared to that observed in galaxies, but one that it is consistent with those seen in nearby clouds. The different slope is a result of the use of a constant CO-to-H-2 conversion factor in the extragalactic studies, which in turn is related to the assumption of constant metallicity in galaxies. We find a linear correlation between the SFR surface density and that of the dense molecular gas.
C1 [Pineda, J. L.; Langer, W. D.; Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pineda, JL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Jorge.Pineda@jpl.nasa.gov
RI Goldsmith, Paul/H-3159-2016; 
OI Goodman, Alyssa/0000-0003-1312-0477
FU National Aeronautics and Space Administration
FX This research was conducted at the Jet Propulsion Laboratory, California
   Institute of Technology under contract with the National Aeronautics and
   Space Administration. We thank the staffs of the ESA and NASA Herschel
   Science Centers for their help. We would like to thank Roberto Assef,
   Moshe Elitzur, Tanio Diaz-Santos, Guillermo Blanc, and Rodrigo
   Herrera-Camus for enlightening discussions. We also thank an anonymous
   referee for a number of useful comments.
NR 87
TC 21
Z9 21
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
   FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2014
VL 570
AR A121
DI 10.1051/0004-6361/201424054
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS3EE
UT WOS:000344158500064
ER

PT J
AU Serra, P
   Lagache, G
   Dore, O
   Pullen, A
   White, M
AF Serra, P.
   Lagache, G.
   Dore, O.
   Pullen, A.
   White, M.
TI Cross-correlation of cosmic far-infrared background anisotropies with
   large scale structures
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE cosmic background radiation; infrared: diffuse background; galaxies:
   evolution; large-scale structure of Universe; galaxies: statistics
ID STAR-FORMING GALAXIES; PHOTOMETRIC LUMINOUS GALAXIES; POWER SPECTRUM
   ANALYSIS; SOUTH-POLE TELESCOPE; DARK-MATTER HALOES; DUST EMISSION;
   SDSS-III; COSMOLOGICAL IMPLICATIONS; SUBMILLIMETER GALAXIES;
   HIGH-REDSHIFT
AB We measure the cross-power spectra between luminous red galaxies (LRGs) from the Sloan Digital Sky Survey (SDSS)-III data release 8 (DR8) and cosmic infrared background (CIB) anisotropies from Planck and data from the Improved Reprocessing (IRIS) of the Infrared Astronomical Satellite (IRAS) at 353, 545, 857, and 3000 GHz, corresponding to 850, 550, 350 and 100 mu m, respectively, in the multipole range 100 < l < 1000. Using approximately 6.5 x 10(5) photometrically determined LRGs in 7760 deg(2) of the northern hemisphere in the redshift range 0.45 < z < 0.65, we model the far-infrared background (FIRB) anisotropies with an extended version of the halo model. With these methods, we confirm the basic picture obtained from recent analyses of FIRB anisotropies with Herschel and Planck that the most efficient halo mass at hosting star forming galaxies is log(M-eff = M-circle dot) = 12.84 +/- 0.15. We estimate the percentage of FIRB anisotropies correlated with LRGs as approximately 11.8%, 3.9%, 1.8%, and 1.0% of the total at 3000, 857, 545, and 353 GHz, respectively. At redshift z similar to 0.55, the bias of FIRB galaxies with respect to the dark matter density field has the value b(FIRB) similar to 1.45, and the mean dust temperature of FIRB galaxies is T-d = 26 K. Finally, we discuss the impact of present and upcoming cross-correlations with far-infrared background anisotropies on the determination of the global star formation history and the link between galaxies and dark matter.
C1 [Serra, P.; Lagache, G.] Univ Paris 11, IAS, F-91405 Orsay, France.
   [Serra, P.; Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France.
   [Dore, O.; Pullen, A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Dore, O.; Pullen, A.] CALTECH, Pasadena, CA 91125 USA.
   [White, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
   [White, M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
RP Serra, P (reprint author), Univ Paris 11, IAS, Bat 121, F-91405 Orsay, France.
EM pserra@ias.u-psud.fr
RI Pullen, Anthony/I-7007-2015; White, Martin/I-3880-2015
OI Pullen, Anthony/0000-0002-2091-8738; White, Martin/0000-0001-9912-5070
FU ESA (France); CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy);
   CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK);
   CSIC (Spain); MICINN (Spain); JA (Spain); Tekes (Finland); AoF
   (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada);
   DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland);
   FCT/MCTES (Portugal); PRACE (EU); National Aeronautics and Space
   Administration
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 and JA (Spain); Tekes, AoF and
   CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark);
   SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES
   (Portugal); and PRACE (EU). A description of the Planck Collaboration
   and a list of its members, including the technical or scientific
   activities in which they have been involved, can be found at
   http://www.sciops.esa.int/index.php?
   project=planck&page=Planck_Collaboration. We would like to thank the
   anonymous referee for providing us with constructive comments and
   suggestions. P.S. would like to thank Alex Amblard and Shirley Ho for
   useful discussions. 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.
NR 77
TC 4
Z9 4
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 OCT
PY 2014
VL 570
AR A98
DI 10.1051/0004-6361/201423958
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS3EE
UT WOS:000344158500057
ER

PT J
AU Freedman, RS
   Lustig-Yaeger, J
   Fortney, JJ
   Lupu, RE
   Marley, MS
   Lodders, K
AF Freedman, Richard S.
   Lustig-Yaeger, Jacob
   Fortney, Jonathan J.
   Lupu, Roxana E.
   Marley, Mark S.
   Lodders, Katharina
TI GASEOUS MEAN OPACITIES FOR GIANT PLANET AND ULTRACOOL DWARF ATMOSPHERES
   OVER A RANGE OF METALLICITIES AND TEMPERATURES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE brown dwarfs; opacity; planets and satellites: atmospheres; radiative
   transfer; stars: atmospheres
ID COLLISION-INDUCED ABSORPTION; MOLECULAR SPECTROSCOPIC DATABASE; MU-M
   SPECTRA; BROWN DWARF; LINE LISTS; HOT JUPITERS; CHEMICAL-EQUILIBRIUM;
   1500 K; IRRADIATED ATMOSPHERES; RADIATIVE EQUILIBRIUM
AB We present new calculations of Rosseland and Planck gaseous mean opacities relevant to the atmospheres of giant planets and ultracool dwarfs. Such calculations are used in modeling the atmospheres, interiors, formation, and evolution of these objects. Our calculations are an expansion of those presented in Freedman et al. to include lower pressures, finer temperature resolution, and also the higher metallicities most relevant for giant planet atmospheres. Calculations span 1 mu bar to 300 bar, and 75-4000 K, in a nearly square grid. Opacities at metallicities from solar to 50 times solar abundances are calculated. We also provide an analytic fit to the Rosseland mean opacities over the grid in pressure, temperature, and metallicity. In addition to computing mean opacities at these local temperatures, we also calculate them with weighting functions up to 7000 K, to simulate the mean opacities for incident stellar intensities, rather than locally thermally emitted intensities. The chemical equilibrium calculations account for the settling of condensates in a gravitational field and are applicable to cloud-free giant planet and ultracool dwarf atmospheres, but not circumstellar disks. We provide our extensive opacity tables for public use.
C1 [Freedman, Richard S.] SETI Inst, Mountain View, CA 94043 USA.
   [Freedman, Richard S.; Lupu, Roxana E.; Marley, Mark S.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
   [Lustig-Yaeger, Jacob] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
   [Lustig-Yaeger, Jacob; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Lodders, Katharina] Washington Univ, Planetary Chem Lab, St Louis, MO USA.
RP Freedman, RS (reprint author), SETI Inst, Mountain View, CA 94043 USA.
EM Richard.S.Freedman@nasa.gov
RI Lupu, Roxana/P-9060-2014; 
OI Lupu, Roxana/0000-0003-3444-5908; Marley, Mark/0000-0002-5251-2943
NR 80
TC 19
Z9 19
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD OCT
PY 2014
VL 214
IS 2
AR 25
DI 10.1088/0067-0049/214/2/25
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS2YE
UT WOS:000344141500011
ER

PT J
AU Skelton, RE
   Whitaker, KE
   Momcheva, IG
   Brammer, GB
   van Dokkum, PG
   Labbe, I
   Franx, M
   van der Wel, A
   Bezanson, R
   Da Cunha, E
   Fumagalli, M
   Schreiber, NF
   Kriek, M
   Leja, J
   Lundgren, BF
   Magee, D
   Marchesini, D
   Maseda, MV
   Nelson, EJ
   Oesch, P
   Pacifici, C
   Patel, SG
   Price, S
   Rix, HW
   Tal, T
   Wake, DA
   Wuyts, S
AF Skelton, Rosalind E.
   Whitaker, Katherine E.
   Momcheva, Ivelina G.
   Brammer, Gabriel B.
   van Dokkum, Pieter G.
   Labbe, Ivo
   Franx, Marijn
   van der Wel, Arjen
   Bezanson, Rachel
   Da Cunha, Elisabete
   Fumagalli, Mattia
   Schreiber, Natascha Foerster
   Kriek, Mariska
   Leja, Joel
   Lundgren, Britt F.
   Magee, Daniel
   Marchesini, Danilo
   Maseda, Michael V.
   Nelson, Erica J.
   Oesch, Pascal
   Pacifici, Camilla
   Patel, Shannon G.
   Price, Sedona
   Rix, Hans-Walter
   Tal, Tomer
   Wake, David A.
   Wuyts, Stijn
TI 3D-HST WFC3-SELECTED PHOTOMETRIC CATALOGS IN THE FIVE CANDELS/3D-HST
   FIELDS: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR MASSES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; galaxies: evolution; galaxies: general; methods: data
   analysis; techniques: photometric
ID HUBBLE-DEEP-FIELD; SIMILAR-TO 2; STAR-FORMING GALAXIES; YALE-CHILE
   MUSYC; SPECTRAL ENERGY-DISTRIBUTIONS; PASSIVELY EVOLVING GALAXIES;
   EXTRAGALACTIC LEGACY SURVEY; EVOLUTION SURVEY COSMOS; EXTENDED GROTH
   STRIP; LYMAN-BREAK GALAXIES
AB The 3D-HST and CANDELS programs have provided WFC3 and ACS spectroscopy and photometry over approximate to 900 arcmin(2) in five fields: AEGIS, COSMOS, GOODS-North, GOODS-South, and the UKIDSS UDS field. All these fields have a wealth of publicly available imaging data sets in addition to the Hubble Space Telescope (HST) data, which makes it possible to construct the spectral energy distributions (SEDs) of objects over a wide wavelength range. In this paper we describe a photometric analysis of the CANDELS and 3D-HST HST imaging and the ancillary imaging data at wavelengths 0.3-8 mu m. Objects were selected in the WFC3 near-IR bands, and their SEDs were determined by carefully taking the effects of the point-spread function in each observation into account. A total of 147 distinct imaging data sets were used in the analysis. The photometry is made available in the form of six catalogs: one for each field, as well as a master catalog containing all objects in the entire survey. We also provide derived data products: photometric redshifts, determined with the EAZY code, and stellar population parameters determined with the FAST code. We make all the imaging data that were used in the analysis available, including our reductions of the WFC3 imaging in all five fields. 3D-HST is a spectroscopic survey with the WFC3 and ACS grisms, and the photometric catalogs presented here constitute a necessary first step in the analysis of these grism data. All the data presented in this paper are available through the 3D-HST Web site (http://3dhst.research.yale.edu).
C1 [Skelton, Rosalind E.] S African Astron Observ, ZA-7935 Cape Town, South Africa.
   [Skelton, Rosalind E.; Momcheva, Ivelina G.; van Dokkum, Pieter G.; Bezanson, Rachel; Leja, Joel; Nelson, Erica J.; Oesch, Pascal] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
   [Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
   [Brammer, Gabriel B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Labbe, Ivo; Franx, Marijn; Fumagalli, Mattia] Leiden Univ, Leiden Observ, Leiden, Netherlands.
   [van der Wel, Arjen; Da Cunha, Elisabete; Maseda, Michael V.; Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Bezanson, Rachel] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
   [Schreiber, Natascha Foerster; Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
   [Kriek, Mariska; Price, Sedona] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Lundgren, Britt F.; Wake, David A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
   [Magee, Daniel; Tal, Tomer] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Marchesini, Danilo] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA.
   [Pacifici, Camilla] Yonsei Univ, Yonsei Univ Observ, Seoul 120749, South Korea.
   [Patel, Shannon G.; Wake, David A.] Carnegie Observ, Pasadena, CA 91101 USA.
   [Wake, David A.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
RP Skelton, RE (reprint author), S African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa.
EM ros@saao.ac.za
RI Skelton, Rosalind/S-1845-2016; 
OI Skelton, Rosalind/0000-0001-7393-3336; Leja, Joel/0000-0001-6755-1315;
   Oesch, Pascal/0000-0001-5851-6649; Price, Sedona/0000-0002-0108-4176; da
   Cunha, Elisabete/0000-0001-9759-4797; Brammer,
   Gabriel/0000-0003-2680-005X
FU South African National Research Foundation; NASA Postdoctoral Program at
   the Goddard Space Flight Center; Research Corporation for Science
   Advancements Cottrell Scholarship; NSF Astronomy and Astrophsics
   Fellowship [AST-1202963]; ERC Advanced Grant HIGHZ [227749]; NWO Spinoza
   Grant; Lorentz Center; NASA [NAS 5-26555]; W. M. Keck Foundation;
   National Aeronautics and Space Administration; NSF; NASA; STFC;
   Smithsonian Astrophysical Observatory
FX We are grateful to the many colleagues who have provided public data and
   catalogs in the five fields described in this paper; high redshift
   galaxy science has thrived owing to this gracious mindset and the TACs
   and Observatory Directors who have encouraged this. Formal
   acknowledgements follow below. R.S. acknowledges the support of the
   South African National Research Foundation through the Professional
   Development Programme Postdoctoral Fellowship. K.W. acknowledges support
   by an appointment to the NASA Postdoctoral Program at the Goddard Space
   Flight Center, administered by Oak Ridge Associated Universities through
   a contract with the National Aeronautics and Space Administration
   (NASA). D.M. acknowledges the support of the Research Corporation for
   Science Advancements Cottrell Scholarship. B.L. acknowledges support
   from the NSF Astronomy and Astrophsics Fellowship grant AST-1202963. We
   acknowledge support from ERC Advanced Grant HIGHZ #227749 and an NWO
   Spinoza Grant. We thank the Lorentz Center for its support and
   hospitality.; This work is based on observations made with the NASA/ESA
   Hubble Space Telescope, obtained from the MAST Data Archive 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. Observations associated with the following GO and GTO programs
   were used: 12063, 12440, 12442, 12443, 12444, 12445, 12060, 12061,
   12062, 12064 (PI: Faber); 12177 and 12328 (PI: van Dokkum); 12461 and
   12099 (PI: Riess); 11600 (PI: Weiner); 9425 and 9583 (PI: Giavalisco);
   12190 (PI: Koekemoer); 11359 and 11360 (PI: OConnell); 11563 (PI:
   Illingworth). Based, in part, on data 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 was made possible by the generous financial support of the W.
   M. Keck Foundation. This work makes use of data obtained as part of the
   ESO/GOODS survey. Observations have been carried out using the Very
   Large Telescope at the ESO Paranal Observatory under Programme ID
   168.A-0485. Based on observations made with ESO Telescopes at the La
   Silla or Paranal Observatories under programme number 168.A-0485. Based
   on data products from observations made with ESO Telescopes at the La
   Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data
   products produced by TERAPIX and the Cambridge Astronomy Survey Unit on
   behalf of the UltraVISTA consortium. Based on observations obtained with
   MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the
   Canada-France-Hawaii Telescope (CFHT) which is operated by the National
   Research Council (NRC) of Canada, the Institut National des Science de
   l'Univers of the Centre National de la Recherche Scientifique (CNRS) of
   France, and the University of Hawaii. This work is based in part on data
   products produced at Terapix available at the Canadian Astronomy Data
   Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a
   collaborative project of NRC and CNRS. This work makes use of data
   products produced at TERAPIX, the WIRDS consortium, and the Canadian
   Astronomy Data Centre. We thank H. Hildebrandt for providing the
   CARS-reduced CFHTLS images. 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. This study makes use of
   data from AEGIS, a multiwavelength sky survey conducted with the
   Chandra, GALEX, Hubble, Keck, CFHT, MMT, Subaru, Palomar, Spitzer, VLA,
   and other telescopes and supported in part by the NSF, NASA, and the
   STFC. This study makes use of data from the NEWFIRM Medium-Band Survey,
   a multi-wavelength survey conducted with the NEWFIRM instrument at the
   KPNO, supported in part by the NSF and NASA. This paper uses data
   products produced by the OIR Telescope Data Center, supported by the
   Smithsonian Astrophysical Observatory. 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
   contract with NASA. Based in part on data from the UKIDSS Ultra Deep
   Survey (UDS) and the Spitzer Public Legacy Survey of the UKIDSS Ultra
   Deep Survey (SpUDS), a Cycle 4 Spitzer Legacy program.
NR 115
TC 129
Z9 130
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD OCT
PY 2014
VL 214
IS 2
AR 24
DI 10.1088/0067-0049/214/2/24
PG 49
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AS2YE
UT WOS:000344141500010
ER

PT J
AU Kim, D
   Lee, MI
   Kim, HM
   Schubert, SD
   Yoo, JH
AF Kim, Dongmin
   Lee, Myong-In
   Kim, Hye-Mi
   Schubert, Siegfried D.
   Yoo, Jin Ho
TI The modulation of tropical storm activity in the Western North Pacific
   by the Madden-Julian Oscillation in GEOS-5 AGCM experiments
SO ATMOSPHERIC SCIENCE LETTERS
LA English
DT Article
DE tropical storms; MJO; GEOS-5; AGCM
ID SUMMER INTRASEASONAL OSCILLATION; EASTERN PACIFIC; CYCLONES; MJO;
   VARIABILITY; CLIMATE; CIRCULATION; SIMULATIONS; MODELS; ENSO
AB This study examines the influence of the Madden-Julian Oscillation (MJO) on tropical storm (TS) activity in the western North Pacific, using observations and GEOS-5 simulations at 50-km horizontal resolution. While GEOS-5 produces an MJO of faster propagation and weaker amplitude, it nevertheless reproduces the observed modulation of TS activity by the MJO with the highest TS genesis and increased track density in the active phases of MJO. The study suggests that the simulation of the sub-seasonal variability of TS activity could be improved by improving the simulations of the MJO in climate models.
C1 [Kim, Dongmin; Lee, Myong-In] Ulsan Natl Inst Sci & Technol, Sch Urban & Environm Engn, Ulsan 689798, South Korea.
   [Kim, Hye-Mi] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
   [Schubert, Siegfried D.] NASA, Goddard Space Flight Ctr, GMAO, Greenbelt, MD 20771 USA.
   [Yoo, Jin Ho] APEC Climate Ctr, Pusan, South Korea.
RP Lee, MI (reprint author), Ulsan Natl Inst Sci & Technol, Sch Urban & Environm Engn, UNIST Gil 50, Ulsan 689798, South Korea.
EM milee@unist.ac.kr
OI Lee, Myong-In/0000-0001-8983-8624
FU APEC Climate Center; NASA Modeling, Analysis and Prediction (MAP)
   Program
FX This study was supported by the APEC Climate Center, and the NASA
   Modeling, Analysis and Prediction (MAP) Program. The authors are
   grateful for the computing resources provided by NASA and the
   Supercomputing Center at Korea Institute of Science and Technology
   Information (KSC-2013-C2-011).
NR 24
TC 2
Z9 2
U1 1
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1530-261X
J9 ATMOS SCI LETT
JI Atmos. Sci. Lett.
PD OCT-DEC
PY 2014
VL 15
IS 4
BP 335
EP 341
DI 10.1002/asl2.509
PG 7
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA AS5WU
UT WOS:000344338200015
ER

PT J
AU Campbell, MD
   Driggers, WB
   Sauls, B
   Walter, JF
AF Campbell, Matthew D.
   Driggers, William B., III
   Sauls, Beverly
   Walter, John F.
TI Release mortality in the red snapper (Lutjanus campechanus) fishery: a
   meta-analysis of 3 decades of research
SO FISHERY BULLETIN
LA English
DT Article
ID GULF-OF-MEXICO; REFLEX IMPAIRMENT; DELAYED MORTALITY; RELATIVE SURVIVAL;
   PACIFIC ROCKFISH; CONDITION INDEX; CATCH; STRESS; MODEL; BAROTRAUMA
AB The value of catch-and-release fishing as a conservation measure is highly dependent upon rates of discard frequency and release mortality. Therefore, it is important to understand how estimates of these variables are affected by factors such as capture depth and water temperature. The meta-analytical approach to modeling used here for red snapper (Lutjanus campechanus) in the Gulf of Mexico provides a robust method for dealing with study-specific differences in experimental protocols and for estimating release (discard) mortality as a function of key factors. Results of this analysis showed significant increases in mortality by depth and for the commercial sector. The most consistent result was the positive correlation between depth and estimates of release mortality, a relationship that was present regardless of study method, fishing sector, hook type used, or season of study. The effect of venting (deflating the swim bladder by puncture) was dependent on whether the study produced estimates of immediate or delayed mortality. Immediate estimates indicated that mortality rates are lowered by venting whereas delayed estimates indicated that venting increased mortality rates. This result is largely reflective of the use of submergence ability, from surface-release studies, as a proxy for mortality. The model's interaction result indicates that recompression of fish may be a viable alternative to venting and that, if a recompression device is not available, venting at least improves the likelihood that a fish can submerge and return to protective habitat. The depth-based functional relationships developed in this model were used in the most recent red snapper stock assessment in 2012, and that use was a change from previous assessments where region-specific point estimates were used.
C1 [Campbell, Matthew D.; Driggers, William B., III] Natl Marine Fisheries Serv, Mississippi Labs, Southeast Fisheries Sci Ctr, NOAA, Pascagoula, MS 39567 USA.
   [Sauls, Beverly] Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, St Petersburg, FL 33701 USA.
   [Walter, John F.] Natl Marine Fisheries Serv, Sustainable Fisheries Div, Southeast Fisheries Sci Ctr, NOAA, Miami, FL 33149 USA.
RP Campbell, MD (reprint author), Natl Marine Fisheries Serv, Mississippi Labs, Southeast Fisheries Sci Ctr, NOAA, 3209 Frederic St, Pascagoula, MS 39567 USA.
EM matthew.d.campbell@noaa.gov
OI Campbell, Matthew/0000-0002-0087-5291
NR 33
TC 4
Z9 4
U1 2
U2 30
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
EI 1937-4518
J9 FISH B-NOAA
JI Fish. Bull.
PD OCT
PY 2014
VL 112
IS 4
BP 283
EP 296
DI 10.7755/FB.112.4.5
PG 14
WC Fisheries
SC Fisheries
GA AS7PY
UT WOS:000344448700005
ER

PT J
AU Cho, Y
   Kim, J
   Kim, T
   Hong, J
   Lee, S
AF Cho, Yoonho
   Kim, Jaehwan
   Kim, Taehyung
   Hong, Jiyoung
   Lee, Soogab
TI Comparative study on civil aircraft noise metrics as annoyance
   estimators for interoperability between other aircraft noise metrics
SO JOURNAL OF MECHANICAL SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Aircraft noise; Annoyance; Energy-averaged noise metrics; Equivalent
   annoyance method; International commission on the biological effects of
   noise; Weighted equivalent continuous perceived noise level
ID TRANSPORTATION NOISE; COMMUNITY ANNOYANCE
AB In Korea, the national noise evaluation system for transportation noise was divided into two kinds of noise metrics: WECPNL (weighted equivalent continuous perceived noise level) for aircraft noise and L (Aeq) for other noises. For administrative and political application of these metrics, a trade-off between them must be maintained. Traditionally, conversion between noise metrics has included correlations between the two metrics based on measured physical quantity. However, conversion between two noise metrics should consider the subjective or emotional aspects of people exposed to noise. In the present study, a field study was conducted in 11 sites in the vicinity of Gimpo airport to propose a rational method to convert Korean WECPNL into DENL (day-evening-night average sound level). Annoyance models for aircraft noise in terms of Korean WECPNL and DENL were established by linear regression analyses for 382 useful data. CBA (conversion based on noise annoyance) was proposed by using the two annoyance models. The validity of the proposed equivalent annoyance method was demonstrated by comparing among dose-response relationships in terms of measured DENL, DENL estimated by the CBA, and DENL estimated by the three empirical relations between WECPNL and DENL.
C1 [Cho, Yoonho; Kim, Taehyung] Seoul Natl Univ, Sch Mech & Aerosp Engn, Seoul, South Korea.
   [Kim, Jaehwan] Seoul Natl Univ, Plus Transformat Training Program Creat Mech & Ae, Seoul, South Korea.
   [Hong, Jiyoung] Korea Railroad Res Inst, Ecosyst Lab, Uiwang, South Korea.
   [Lee, Soogab] Seoul Natl Univ, Engn Res Inst, Seoul, South Korea.
   [Cho, Yoonho; Lee, Soogab] Seoul Natl Univ, Seoul, South Korea.
   [Lee, Soogab] NASA, Ames Res Ctr, Washington, DC USA.
   [Lee, Soogab] Seoul Natl Univ, Dept Mech & Aerosp Engn, Seoul, South Korea.
RP Lee, S (reprint author), Seoul Natl Univ, Engn Res Inst, Gwanak Ro 1, Seoul, South Korea.
EM solee@snu.ac.kr
FU Brain Korea 21 Plus Project; Korea Ministry of Environment (MOE)
FX This work was supported by the Brain Korea 21 Plus Project in 2014. This
   study was funded by the Korea Ministry of Environment (MOE) as "the
   Environmental Health Action Program".
NR 16
TC 0
Z9 0
U1 0
U2 1
PU KOREAN SOC MECHANICAL ENGINEERS
PI SEOUL
PA KSTC NEW BLD. 7TH FLOOR, 635-4 YEOKSAM-DONG KANGNAM-KU, SEOUL 135-703,
   SOUTH KOREA
SN 1738-494X
EI 1976-3824
J9 J MECH SCI TECHNOL
JI J. Mech. Sci. Technol.
PD OCT
PY 2014
VL 28
IS 10
BP 3997
EP 4003
DI 10.1007/s12206-014-0912-x
PG 7
WC Engineering, Mechanical
SC Engineering
GA AS3GC
UT WOS:000344164400012
ER

PT J
AU Huang, LG
   Armbrust, O
AF Huang, LiGuo
   Armbrust, Ove
TI Special Issue: International Conference on Software and System Process
   (ICSSP) 2012 Introduction
SO JOURNAL OF SOFTWARE-EVOLUTION AND PROCESS
LA English
DT Editorial Material
DE Process; ICSSP; Software Systems Engineering
C1 [Huang, LiGuo] So Methodist Univ, Dallas, TX 75275 USA.
   [Armbrust, Ove] NASA Goddard Space Flight Ctr, Telophase Corp, Greenbelt, MD USA.
RP Huang, LG (reprint author), So Methodist Univ, Dallas, TX 75275 USA.
EM lghuang@smu.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2047-7473
EI 2047-7481
J9 J SOFTW-EVOL PROC
JI J. Softw.-Evol. Proc.
PD OCT
PY 2014
VL 26
IS 10
SI SI
BP 867
EP 868
DI 10.1002/smr.1692
PG 2
WC Computer Science, Software Engineering
SC Computer Science
GA AS3AR
UT WOS:000344148200001
ER

PT J
AU Gounelle, M
   Zolensky, ME
AF Gounelle, Matthieu
   Zolensky, Michael E.
TI The Orgueil meteorite: 150 years of history
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID INNER SOLAR-SYSTEM; CARBONACEOUS CHONDRITES; ISOTOPIC COMPOSITION; CI
   CHONDRITES; AQUEOUS ACTIVITY; PARENT BODY; ORGANIZED ELEMENTS; HYDROUS
   ASTEROIDS; COMET 81P/WILD-2; AMINO-ACIDS
AB The goal of this paper is to summarize 150yr of history of a very special meteorite. The Orgueil meteorite fell near Montauban in southwestern France on May 14, 1864. The bolide, which was the size of the full Moon, was seen across Western France, and almost immediately made the news in local and Parisian newspapers. Within a few weeks of the fall, a great diversity of analyses were performed under the authority of Gabriel Auguste Daubree, geology professor at the Paris Museum, and published in the Comptes Rendus de l'Academie des Sciences. The skilled scientists reported the presence of iron sulfides, hydrated silicates, and carbonates in Orgueil. They also characterized ammonium salts which are now gone, and observed sulfates being remobilized at the surface of the stone. They identified the high water and carbon contents, and noted similarities with the Alais meteorite, which had fallen in 1806, 300km away. While Daubree and his colleagues noted the similarity of the Orgueil organic matter with some terrestrial humus, they were cautious not to make a direct link with living organisms. One century later, Nagy and Claus were less prudent and announced the discovery of organized elements in some samples of Orgueil. Their observations were quickly discredited by Edward Anders and others who also discovered that some pollen grains were intentionally placed into the rock back in the 1860s. Orgueil is now one of the most studied meteorites, indeed one of the most studied rocks of any kind. Not only does it contain a large diversity of carbon-rich compounds, which help address the question of organo-synthesis in the early solar system but its chemical composition is also close to that of the Sun's photosphere and serves as a cosmic reference. Secondary minerals, which make up 99% of the volume of Orgueil, were probably formed during hydrothermal alteration on the parent-body within the first few million years of the solar system; their study is essential to our understanding of fluid-rock interaction in asteroids and comets. Finally, the Orgueil meteorite probably originated from a volatile-rich cometary outer solar system body as indicated by its orbit. Because it bears strong similarities to other carbonaceous chondrites that originated on dark asteroids, this cometary connection supports the idea of a continuum between dark asteroids and comets.
C1 [Gounelle, Matthieu] UPMC, Univ Paris 04, Museum Natl Hist Nat, IMPMC, F-75005 Paris, France.
   [Gounelle, Matthieu] IRD, F-75005 Paris, France.
   [Gounelle, Matthieu] Inst Univ France, F-75005 Paris, France.
   [Zolensky, Michael E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Gounelle, M (reprint author), UPMC, Univ Paris 04, Museum Natl Hist Nat, IMPMC, 57 Rue Cuvier, F-75005 Paris, France.
EM gounelle@mnhn.fr
FU NASA; Institut Universitaire de France
FX We thank Florence Greffe, Amelia Laurenceau, and Aude Bergeret for
   providing images or other historical sources. Louis-Dominique Bayle
   kindly authorized us to use his beautiful pictures of Orgueil's
   specimens. Individuals at the Archives municipals et departementales at
   Montauban were extremely welcoming and helpful. John Wood provided most
   interesting information on the comparison of the Orgueil meteorite to
   the Sun photosphere, while Roger Hewins gave us the so far ultimate clue
   on that matter. Jerome Gattacceca guided us in the magnetic experiments
   performed in 1864 by his paleomagnetic pals Laroque and Bianchi. Queenie
   Hoi Shan Chan provided valuable insights into organic chemistry, and we
   have made considerable use of her recent summary of organic analyses of
   Orgueil. Two reviewers, William Hartmann and Emma Bullock, significantly
   helped to improve the paper. We are grateful to Emmanuel Jacquet who
   kindly provided German translations. Finally, we thank Tim Jull, MAPS
   editor, who gave profound insights and made the review process as swift
   as possible. MZ acknowledges the support of NASA's late, great
   Cosmochemistry Program, while MG is grateful to the Institut
   Universitaire de France for its funding and the freedom it allows.
NR 127
TC 4
Z9 4
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 2014
VL 49
IS 10
BP 1769
EP 1794
DI 10.1111/maps.12351
PG 26
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AS0MT
UT WOS:000343972000003
ER

PT J
AU Shi, JJ
   Matsui, T
   Tao, WK
   Tan, Q
   Peters-Lidard, C
   Chin, M
   Pickering, K
   Guy, N
   Lang, S
   Kemp, EM
AF Shi, J. J.
   Matsui, T.
   Tao, W. -K.
   Tan, Q.
   Peters-Lidard, C.
   Chin, M.
   Pickering, K.
   Guy, N.
   Lang, S.
   Kemp, E. M.
TI Implementation of an aerosol-cloud-microphysics-radiation coupling into
   the NASA unified WRF: Simulation results for the 6-7 August 2006 AMMA
   special observing period
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE WRF; AMMA; aerosol; micropysics; radiation
ID WEST-AFRICAN MONSOON; CONVECTIVE SYSTEMS; MODEL DESCRIPTION; FIELD
   EXPERIMENT; DUST AEROSOLS; SAHARAN DUST; GLOBAL-MODEL; PART I;
   SATELLITE-OBSERVATIONS; SUMMER MONSOON
AB Aerosols affect the Earth's radiation balance directly and cloud microphysical processes indirectly via the activation of cloud condensation and ice nuclei. These two effects have often been considered separately and independently, hence the need to assess their combined impact given the differing nature of their effects on convective clouds. To study both effects, an aerosol-microphysics-radiation coupling, including Goddard microphysics and radiation schemes, was implemented into the NASA Unified Weather Research and Forecasting model (NU-WRF). Fully coupled NU-WRF simulations were conducted for a mesoscale convective system (MCS) that passed through the Niamey, Niger area on 6-7 August 2006 during an AMMA special observing period. The results suggest that rainfall is reduced when aerosol indirect effects are included, regardless of the aerosol direct effect. Daily mean radiation heating profiles in the area traversed by the MCS showed the aerosol (mainly mineral dust) direct effect had the largest impact near cloud tops just above 200 hPa where short-wave heating increased by about 0.8 K day(-1); the weakest long-wave cooling was at around 250 hPa. It was also found that more condensation and ice nuclei as a result of higher aerosol/dust concentrations led to increased amounts of all cloud hydrometeors because of the microphysical indirect effect, and the radiation direct effect acts to reduce precipitating cloud particles (rain, snow and graupel) in the middle and lower cloud layers while increasing the non-precipitating particles (ice) in the cirrus anvil. However, when the aerosol direct effect was activated, regardless of the indirect effect, the onset of MCS precipitation was delayed about 2 h, in conjunction with the delay in the activation of cloud condensation and ice nuclei. Overall, for this particular environment, model set-up and physics configuration, the effect of aerosol radiative heating due to mineral dust overwhelmed the effect of the aerosols on microphysics.
C1 [Shi, J. J.; Matsui, T.; Tao, W. -K.; Tan, Q.; Peters-Lidard, C.; Chin, M.; Pickering, K.; Lang, S.; Kemp, E. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Shi, J. J.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA.
   [Matsui, T.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
   [Tan, Q.] Univ Space Res Assoc, Columbia, MD USA.
   [Guy, N.; Kemp, E. M.] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA.
   [Lang, S.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Shi, JJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM jainn.j.shi@nasa.gov
RI Pickering, Kenneth/E-6274-2012; Peters-Lidard, Christa/E-1429-2012;
   Measurement, Global/C-4698-2015; Chin, Mian/J-8354-2012
OI Peters-Lidard, Christa/0000-0003-1255-2876; 
FU NASA headquarters Modeling, Analysis, and Prediction (MAP) Program and
   Interdisciplinary Sciences (IDS) Program
FX This research effort is supported by the NASA headquarters Modeling,
   Analysis, and Prediction (MAP) Program and Interdisciplinary Sciences
   (IDS) Program. The authors are grateful to David Considine at NASA
   headquarters for his support of this research. The authors appreciate
   Kyu-Myong Kim of NASA GSFC and Morgan State University for his help on
   the data analysis. The authors also appreciate the useful discussion
   with Zhining Tao of USRA, Xiaowen Li of NASA GSFC and Morgan State
   University, and Shujia Zhou and Philip Hayes of Northrop Grumman
   Corporation.
NR 83
TC 10
Z9 10
U1 0
U2 11
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD OCT
PY 2014
VL 140
IS 684
BP 2158
EP 2175
DI 10.1002/qj.2286
PN A
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS6WN
UT WOS:000344400200006
ER

PT J
AU Geogdzhayev, I
   Cairns, B
   Mishchenko, MI
   Tsigaridis, K
   van Noije, T
AF Geogdzhayev, Igor
   Cairns, Brian
   Mishchenko, Michael I.
   Tsigaridis, Kostas
   van Noije, Twan
TI Model-based estimation of sampling-caused uncertainty in aerosol remote
   sensing for climate research applications
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE tropospheric aerosols; satellite remote sensing; climate change; aerosol
   climatology; long-term variability
ID UNIFIED SATELLITE CLIMATOLOGY; OPTICAL DEPTH PRODUCT; DATA ASSIMILATION;
   MACC REANALYSIS; MODIS; RETRIEVAL; OCEAN; MISR; THICKNESS; AERONET
AB To evaluate the effect of sampling frequency on the global monthly mean aerosol optical thickness (AOT), we use 6 years of geographical coordinates of Moderate Resolution Imaging Spectroradiometer (MODIS) L2 aerosol data, daily global aerosol fields generated by the Goddard Institute for Space Studies General Circulation Model and the chemical transport models Global Ozone Chemistry Aerosol Radiation and Transport, Spectral Radiation-transport Model for Aerosol Species and Transport Model 5, at a spatial resolution between 1.125 degrees x 1.125 degrees and 2 degrees x 3 degrees: the analysis is restricted to 60 degrees S-60 degrees N geographical latitude. We found that, in general, the MODIS coverage causes an underestimate of the global mean AOT over the ocean. The long-term mean absolute monthly difference between all and dark target (DT) pixels was 0.01-0.02 over the ocean and 0.03-0.09 over the land, depending on the model dataset. Negative DT biases peak during boreal summers, reaching 0.07-0.12 (30-45% of the global long-term mean AOT). Addition of the Deep Blue pixels tempers the seasonal dependence of the DT biases and reduces the mean AOT difference over land by 0.01-0.02. These results provide a quantitative measure of the effect the pixel exclusion due to cloud contamination, ocean sun-glint and land type has on the MODIS estimates of the global monthly mean AOT. We also simulate global monthly mean AOT estimates from measurements provided by pixel-wide along-track instruments such as the Aerosol Polarimetry Sensor and the Cloud-Aerosol LiDAR with Orthogonal Polarization. We estimate the probable range of the global AOT standard error for an along-track sensor to be 0.0005-0.0015 (ocean) and 0.0029-0.01 (land) or 0.5-1.2% and 1.1-4% of the corresponding global means. These estimates represent errors due to sampling only and do not include potential retrieval errors. They are smaller than or comparable to the published estimate of 0.01 as being a climatologically significant change in the global mean AOT, suggesting that sampling density is unlikely to limit the use of such instruments for climate applications at least on a global, monthly scale.
C1 [Geogdzhayev, Igor; Tsigaridis, Kostas] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
   [Geogdzhayev, Igor; Cairns, Brian; Mishchenko, Michael I.; Tsigaridis, Kostas] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
   [van Noije, Twan] Royal Netherlands Meteorol Inst KNMI Climate Res, De Bilt, Netherlands.
RP Geogdzhayev, I (reprint author), Columbia Univ, 2880 Broadway, New York, NY 10025 USA.
EM igor.v.geogdzhayev@nasa.gov
RI Mishchenko, Michael/D-4426-2012; 
OI Cairns, Brian/0000-0002-1980-1022
FU NASA Glory Mission Project
FX We are grateful to Dr Thomas Diehl for providing GOCART data and to Dr
   Toshihiko Takemura for providing SPRINTARS data for this study as well
   as to Li Liu for help with the MODIS Level-2 data. We thank four
   anonymous reviewers whose insightful comments have resulted in a much
   improved article. This study was supported by the research division of
   the NASA Glory Mission Project managed by Hal Maring.
NR 53
TC 3
Z9 3
U1 1
U2 11
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD OCT
PY 2014
VL 140
IS 684
BP 2353
EP 2363
DI 10.1002/qj.2305
PN A
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS6WN
UT WOS:000344400200022
ER

PT J
AU Goguen, JD
AF Goguen, Jay D.
TI Planetary surface photometry and imaging: progress and perspectives
SO REPORTS ON PROGRESS IN PHYSICS
LA English
DT Review
DE planets; imaging; photometry; spectroscopy; polarization; asteroids;
   planetary satellites
ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; MARKOV-CHAIN FORMALISM;
   INDEPENDENTLY SCATTERING PARTICLES; DISCRETE-DIPOLE APPROXIMATION;
   VECTOR RADIATIVE-TRANSFER; ICY GALILEAN SATELLITES; LIGHT-SCATTERING;
   OPTICAL-PROPERTIES; AGGREGATE PARTICLES; ELECTROMAGNETIC SCATTERING
AB Spacecraft have visited and returned many thousands of images and spectra of all of the planets, many of their moons, several asteroids, and a few comet nuclei during the golden age of planetary exploration. The signal in each pixel of each image or spectral channel is a measurement of the radiance of scattered sunlight into a specific direction. The information on the structure and composition of the surface that is contained in variation of the radiance with scattering geometry and wavelength, including polarization state, has only just begun to be exploited and is the topic of this review. The uppermost surfaces of these bodies are mainly composed of particles that are continuously generated by impacts of micrometeoroids and larger impactors. Models of light scattering by distributions of sizes and irregular shapes of particles and by closely packed particles within a surface are challenging. These are active topics of research where considerable progress has recently been made. We focus on the surfaces of bodies lacking atmospheres.
   These surfaces are diverse and their morphologies give evidence of their evolution by impacts and resurfacing by a variety of processes including down slope movement and electrostatic transport of particles, gravitational accumulation of debris, volatile outgassing and migration, and magnetospheric interactions. Sampling of scattering geometries and spatial resolution is constrained by spacecraft trajectories. However, the large number of archived images and spectra demand more quantitative interpretation. The scattering geometry dependence of the radiance is underutilized and promises constraints on the compositions and structure of the surface for materials that lack diagnostic wavelength dependence. The general problem is considered in terms of the lunar regolith for which samples have been returned to Earth.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Goguen, JD (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-401,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Jay.D.Goguen@jpl.nasa.gov
FU NASA; ESA; JAXA
FX The author would like to thank Bruce Hapke and Michael Mishchenko for
   permission to reproduce figures from their papers and two anonymous
   referees for their careful reviews that improved the manuscript. Of
   course, the spectacular images that grace this paper and the background
   knowledge that supports this review exist only as a result of the
   generous public funding of the planetary exploration missions and
   analysis of their data supported by NASA, ESA, JAXA, and other
   international science agencies.
NR 137
TC 1
Z9 1
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0034-4885
EI 1361-6633
J9 REP PROG PHYS
JI Rep. Prog. Phys.
PD OCT
PY 2014
VL 77
IS 10
AR 104901
DI 10.1088/0034-4885/77/10/104901
PG 23
WC Physics, Multidisciplinary
SC Physics
GA AS2YJ
UT WOS:000344142000003
PM 25313169
ER

PT J
AU Van Zante, DE
   Collier, F
   Orton, A
   Khalid, SA
   Wojno, JP
   Wood, TH
AF Van Zante, D. E.
   Collier, F.
   Orton, A.
   Khalid, S. Arif
   Wojno, J. P.
   Wood, T. H.
TI Progress in open rotor propulsors: The FAA/GE/NASA open rotor test
   campaign
SO AERONAUTICAL JOURNAL
LA English
DT Article
ID UNDUCTED FAN
AB Model scale tests of modem 'open rotor' propulsor concepts that have potential for significant fuel burn reduction for aircraft applications were completed at NASA Glenn Research Center. The recent test campaign was a collaboration between NASA, FAA, and General Electric (GE). GE was the primary industrial partner, but other organisations were involved such as Boeing and Airbus who provided additional hardware for fuselage simulations. The open rotor is a modem version of the UnDucted Fan (UDF (R)) that was flight tested in the late 1980s through a partnership between NASA and GE. The UDF (R) was memorable for its scimitar shaped Propeller blades and its unique noise signature. Design methods of the time were not able to optimise for both high aerodynamic efficiency and low noise simultaneously. Contemporary CFD/CAA based design methods can produce open rotor blade designs that maintain efficiency with acceptable acoustic signatures. Tests of two generations of new open rotor designs were conducted in the 9' x 15' Low Speed Wind Tunnel and the 8' x 6' Supersonic Wind Tunnel starting in late 2009 and completed in early 2012. Aerodynamic performance and acoustic data were obtained for take-off, approach and cruise conditions in isolated and semi-installed configurations. Additional detailed flow diagnostic measurements and acoustic
C1 [Van Zante, D. E.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
   [Collier, F.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
   [Orton, A.] FAA, Washington, DC USA.
   [Khalid, S. Arif; Wojno, J. P.] Gen Elect Aviat, Cincinnati, OH USA.
   [Wood, T. H.] Gen Elect Global Res, Niskayuna, NY USA.
RP Van Zante, DE (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM dale.e.vanzante@nasa.gov
FU FAA's NextGen; CLEEN Program
FX This body of work was the result of much hard work and a very successful
   collaboration between GE, FAA, and NASA Environmentally Responsible
   Aviation and Subsonic Fixed Wing Projects. The wind-tunnel crew worked
   tirelessly for the duration of the test. Chris Hughes of the GRC
   Acoustics Branch deserves credit for the ORPR rig refabrication and the
   upfront test planning which set the stage for a successful effort. FAA's
   NextGen and CLEEN Program are reconised for their share and support of
   this program.
NR 24
TC 4
Z9 4
U1 2
U2 6
PU ROYAL AERONAUTICAL SOC
PI LONDON
PA 4 HAMILTON PL, LONDON W1J 7BQ, ENGLAND
SN 0001-9240
J9 AERONAUT J
JI Aeronaut. J.
PD OCT
PY 2014
VL 118
IS 1208
BP 1181
EP 1213
PG 33
WC Engineering, Aerospace
SC Engineering
GA AR7TS
UT WOS:000343783300006
ER

PT J
AU Garai, A
   Kleissl, J
   Sarkar, S
AF Garai, Anirban
   Kleissl, Jan
   Sarkar, Sutanu
TI Flow and heat transfer in convectively unstable turbulent channel flow
   with solid-wall heat conduction
SO JOURNAL OF FLUID MECHANICS
LA English
DT Article
DE atmospheric flows; buoyancy-driven instability; convection
ID ATMOSPHERIC SURFACE-LAYER; DIRECT NUMERICAL-SIMULATION; BOUNDARY-LAYER;
   DOPPLER LIDAR; TEMPERATURE; STATISTICS; VELOCITY; FLUX; PROFILES;
   VORTICES
AB Most turbulent coherent structures in a convectively unstable atmospheric boundary layer are caused by or manifested in ascending warm fluid and descending cold fluids. These structures not only cause ramps in the air temperature timeseries, but also imprint on the underlying solid surface as surface temperature fluctuations. The coupled flow and heat transport mechanism was examined through direct numerical simulation (DNS) of a channel flow allowing for realistic solid-fluid thermal coupling. The thermal activity ratio (TAR; the ratio of thermal inertias of fluid and solid), and the thickness of the solid domain were found to affect the solid-fluid interfacial temperature variations. The solid-fluid interface with large (small) thermal activity ration behaves as an isoflux (isothermal) boundary. For the range of parameters considered here (Grashof number, Gr = 3 * 10(5)-325 * 10(5); TAR = 0.01-1; solid thickness normalized by heat penetration depth = 0.01-10), the solid thermal properties and thickness influence the fluid temperature only in the viscous or conduction region while the convective forcing influences the turbulent flow. Flow structures influence the interfacial temperature more effectively with increasing TAR and solid thickness compared with a constant temperature boundary condition. The change of channel flow structures with increasing convective instability is examined and the concomitant change of thermal patterns is quantified. Despite large differences in friction Reynolds and Richardson number between the DNS and atmospheric observations, similarities in the flow features were observed.
C1 [Garai, Anirban; Kleissl, Jan; Sarkar, Sutanu] Univ Calif San Diego, Dept Mech & Aerosp Engn, San Diego, CA 92093 USA.
RP Garai, A (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jkleissl@ucsd.edu
FU NASA; National Science Foundation [OCI-1053575]; State of Wyoming;
   National Center for Atmospheric Research's (NCAR) Computational and
   Information System Laboratory
FX We are grateful to (i) NASA for funding through a New Investigator
   Program award, (ii) the NCAR-Wyoming Supercomputer Center (funded by the
   National Science Foundation and the State of Wyoming) which is supported
   by National Center for Atmospheric Research's (NCAR) Computational and
   Information System Laboratory and (iii) San Diego Supercomputer Center,
   Extreme Science and Engineering Discovery Environment (XSEDE) program,
   which is supported by National Science Foundation grant number
   OCI-1053575 for providing computing resources.
NR 64
TC 4
Z9 4
U1 2
U2 12
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 OCT
PY 2014
VL 757
BP 57
EP 81
DI 10.1017/jfm.2014.479
PG 25
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA AR7KB
UT WOS:000343757200004
ER

PT J
AU Schakner, ZA
   Lunsford, C
   Straley, J
   Eguchi, T
   Mesnick, SL
AF Schakner, Zachary A.
   Lunsford, Chris
   Straley, Janice
   Eguchi, Tomoharu
   Mesnick, Sarah L.
TI Using Models of Social Transmission to Examine the Spread of Longline
   Depredation Behavior among Sperm Whales in the Gulf of Alaska
SO PLOS ONE
LA English
DT Article
ID ACCELERATING LEARNING RATES; PHYSETER-MACROCEPHALUS; CULTURAL
   TRANSMISSION; DIFFUSION DYNAMICS; FISHERIES
AB Fishing, farming and ranching provide opportunities for predators to prey on resources concentrated by humans, a behavior termed depredation. In the Gulf of Alaska, observations of sperm whales depredating on fish caught on demersal longline gear dates back to the 1970s, with reported incidents increasing in the mid-1990s. Sperm whale depredation provides an opportunity to study the spread of a novel foraging behavior within a population. Data were collected during National Marine Fisheries Service longline surveys using demersal longline gear in waters off Alaska from 1998 to 2010. We evaluated whether observations of depredation fit predictions of social transmission by fitting the temporal and spatial spread of new observations of depredation to the Wave of Advance model. We found a significant, positive relationship between time and the distance of new observations from the diffusion center (r(2) = 0.55, p-value = 0.003). The data provide circumstantial evidence for social transmission of depredation. We discuss how changes in human activities in the region (fishing methods and regulations) have created a situation in which there is spatial-temporal overlap with foraging sperm whales, likely influencing when and how the behavior spread among the population.
C1 [Schakner, Zachary A.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
   [Lunsford, Chris] Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, NOAA, Auke Bay Labs, Juneau, AK USA.
   [Straley, Janice] Univ Alaska Southeast, Sitka, AK USA.
   [Eguchi, Tomoharu; Mesnick, Sarah L.] Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, NOAA, La Jolla, CA 92038 USA.
RP Schakner, ZA (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
EM zschakner@ucla.edu; sarah.mesnick@noaa.gov
FU National Science Foundation
FX Z.A.S. is supported by a National Science Foundation Graduate Research
   Fellowship. The funder had no role in study design, data collection and
   analysis, decision to publish, or preparation of the manuscript.
NR 25
TC 4
Z9 4
U1 2
U2 18
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD OCT 1
PY 2014
VL 9
IS 10
AR e109079
DI 10.1371/journal.pone.0109079
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AR6ZM
UT WOS:000343729600097
PM 25272019
ER

PT J
AU Johnson, K
   Brown, ME
AF Johnson, Kiersten
   Brown, Molly E.
TI Environmental risk factors and child nutritional status and survival in
   a context of climate variability and change
SO APPLIED GEOGRAPHY
LA English
DT Article
DE NDVI; Stunting; Mortality; Nutrition; Child survival; West Africa
ID SUB-SAHARAN AFRICA; FOOD SECURITY; NOAA-AVHRR; SPOT-VEGETATION;
   WEST-AFRICA; NDVI DATA; RAINFALL; BIOMASS; SAHEL; IMPACT
AB Much of the population in the developing world resides in rural areas, is dependent on local agriculture for survival, and thus directly subject to increasingly volatile and variable climatic patterns. Poverty limits options for adaptation to unpredictable weather and resultant food insecurity; these concerns are particularly salient in an era of climate change, which threatens to roll back years of development gains. Examining the association between the growing environment and child survival and nutrition is important in this context. Using NASA's satellite remote sensing data with Demographic and Health Surveys (DHS) data from four West African countries (Mali, Burkina Faso, Guinea and Benin), we assess the association between a climate-related environmental variable (vegetation index - NDVI) and child survival and nutrition. NDVI had a positive association with child survival and nutrition in countries with a wide distribution of NDVI values. NDVI was more likely to be positively associated with wasting rather than stunting. We find that environmental factors can be important for child survival and nutrition outcomes in specific contexts. Additional research is needed to further explore the ways NDVI can be used to inform our understanding of the environment's impact on child survival and nutrition. (C) 2014 Published by Elsevier Ltd.
C1 [Johnson, Kiersten] WESTAT Corp, Rockville, MD 20850 USA.
   [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
RP Brown, ME (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 614-4, Greenbelt, MD 20771 USA.
EM kierstenjohnson@westat.com; mebrown69@gmail.com
RI Brown, Molly/E-2724-2010
OI Brown, Molly/0000-0001-7384-3314
NR 79
TC 2
Z9 2
U1 2
U2 29
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0143-6228
EI 1873-7730
J9 APPL GEOGR
JI Appl. Geogr.
PD OCT
PY 2014
VL 54
SI SI
BP 209
EP 221
DI 10.1016/j.apgeog.2014.08.007
PG 13
WC Geography
SC Geography
GA AR6JM
UT WOS:000343689900020
ER

PT J
AU Kelsey, CR
   Scott, JM
   Lane, A
   Schwitzer, E
   West, MJ
   Thomas, S
   Herndon, JE
   Michalski, MG
   Horwitz, ME
   Hennig, T
   Jones, LW
AF Kelsey, C. R.
   Scott, J. M.
   Lane, A.
   Schwitzer, E.
   West, M. J.
   Thomas, S.
   Herndon, J. E., II
   Michalski, M. G.
   Horwitz, M. E.
   Hennig, T.
   Jones, L. W.
TI Cardiopulmonary exercise testing prior to myeloablative allo-SCT: a
   feasibility study
SO BONE MARROW TRANSPLANTATION
LA English
DT Article
ID STEM-CELL TRANSPLANTATION; TOTAL-BODY IRRADIATION; VENTRICULAR EJECTION
   FRACTION; BONE-MARROW-TRANSPLANTATION; MAXIMAL AEROBIC CAPACITY;
   PULMONARY-FUNCTION TESTS; PEAK OXYGEN-CONSUMPTION; LUNG-CANCER;
   PREDICTIVE-VALUE; FUNCTIONAL-CAPACITY
AB The feasibility of symptom-limited cardiopulmonary exercise testing (CPET) prior to allo-SCT was assessed in addition to the prognostic value of CPET-derived measures. CPET was performed prospectively on 21 patients with hematologic malignancies, with assessments of peak (for example, peak oxygen consumption, VO2peak) and submaximal (for example, ventilatory threshold (VT)) measures of cardiopulmonary function. No serious adverse events were observed during CPET procedures, with 95% of patients achieving criteria for a peak test. Mean VO2peak was 24.7 +/- 6.4 mL kg(-1) min(-1) (range: 10.9-35.5), equivalent to 29% +/- 17% below that of age-matched healthy controls. All patients proceeded with the conditioning regimen followed by allo-SCT. Median follow-up was 25 months. During this period, 11 (52.4%) patients died (n = 6, relapsed disease; n = 5, non-relapse mortality (NRM)); 9 patients (43%) developed pulmonary toxicity. In univariate analyses, both peak and submaximal markers of cardiopulmonary function were predictors of OS, pulmonary toxicity and NRM. For OS, the HR for VO2peak and VT were 0.89 (95% CI, 0.8-0.99, P = 0.04) and 0.84 (95% CI, 0.71-0.98, P = 0.03), respectively. In conclusion, CPET is safe and feasible prior to allo-SCT. Patients have marked impairments in cardiopulmonary function prior to allo-SCT. CPET-derived metrics may complement conventional measures to improve risk stratification.
C1 [Kelsey, C. R.; Lane, A.; Schwitzer, E.; West, M. J.; Thomas, S.; Herndon, J. E., II; Michalski, M. G.; Horwitz, M. E.; Hennig, T.] Duke Univ, Med Ctr, Dept Radiat Oncol, Durham, NC 27710 USA.
   [Scott, J. M.] Univ Space Res Assoc, NASA, Johnson Space Ctr, Houston, TX USA.
   [Jones, L. W.] Mem Sloan Kettering Canc Ctr, New York, NY 10021 USA.
RP Kelsey, CR (reprint author), Duke Univ, Med Ctr, Dept Radiat Oncol, DUMC Box 3085, Durham, NC 27710 USA.
EM christopher.kelsey@duke.edu
FU National Cancer Institute
FX LWJ is supported in part by research grants from the National Cancer
   Institute.
NR 42
TC 10
Z9 10
U1 0
U2 1
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0268-3369
EI 1476-5365
J9 BONE MARROW TRANSPL
JI Bone Marrow Transplant.
PD OCT
PY 2014
VL 49
IS 10
BP 1330
EP 1336
DI 10.1038/bmt.2014.159
PG 7
WC Biophysics; Oncology; Hematology; Immunology; Transplantation
SC Biophysics; Oncology; Hematology; Immunology; Transplantation
GA AR5ZC
UT WOS:000343660300014
PM 25068429
ER

PT J
AU Filacchione, G
   Ciarniello, M
   Capaccioni, F
   Clark, RN
   Nicholson, PD
   Hedman, MM
   Cuzzi, JN
   Cruikshank, DP
   Ore, CMD
   Brown, RH
   Cerroni, P
   Altobelli, N
   Spilker, LJ
AF Filacchione, G.
   Ciarniello, M.
   Capaccioni, F.
   Clark, R. N.
   Nicholson, P. D.
   Hedman, M. M.
   Cuzzi, J. N.
   Cruikshank, D. P.
   Ore, C. M. Dalle
   Brown, R. H.
   Cerroni, P.
   Altobelli, N.
   Spilker, L. J.
TI Cassini-VIMS observations of Saturn's main rings: I. Spectral properties
   and temperature radial profiles variability with phase angle and
   elevation
SO ICARUS
LA English
DT Article
DE Saturn, rings; Spectroscopy; Ices
ID INFRARED MAPPING SPECTROMETER; PARTICULATE SURFACES; THERMAL
   OBSERVATIONS; ICY SATELLITES; DARK MATERIAL; IAPETUS; SYSTEM; MODEL;
   PARTICLES; EMISSION
AB The spectral properties and thermal behavior of Saturn's rings are determined from a dataset of ten radial mosaics acquired by Cassini-VIMS (Visual and Infrared Mapping Spectrometer) between October 29th 2004 and January 27th 2010 with phase angle ranging between 5.7 degrees and 132.4 degrees and elevation angles between -23.5 degrees and 2.6 degrees. These observations, after reduction to spectrograms, e.g. 2D arrays containing the VIS-IR (0.35-5.1 mu m) spectral information versus radial distance from Saturn (from 73.500 to 141.375 km, 400 km/bin), allow us to compare the derived spectral and thermal properties of the ring particles on a common reference. Spectral properties: rings spectra are characterized by an intense reddening at visible wavelengths while they maintain a strong similarity with water ice in the infrared domain. Significant changes in VIS reddening, water ice abundance and grain sizes are observed across different radial regions resulting in correlation with optical depth and local structures. The availability of observations taken at very different phase angles allows us to examine spectrophotometric properties of the ring's particles. When observed at high phase angles, a remarkable increase of visible reddening and water ice band depths is found, probably as a consequence of the presence of a red-colored contaminant intimately mixed within water ice grains and of multiple scattering. At low phases the analysis of the 3.2-3.6 mu m range shows faint spectral signatures at 3.42-3.52 mu m which are compatible with the CH2 aliphatic stretch. The 3.29 mu m PAH aromatic stretch absorption is not clearly detectable on this dataset. VIMS results indicate that ring particles contain about 90-95% water ice while the remaining 5-10% is consistent with different contaminants like amorphous carbon or tholins. However, we cannot exclude the presence of nanophase iron or hematite produced by iron oxidation in the rings tenuous oxygen atmosphere, intimately mixed with the ice grains. Greater pollution caused by meteoritic material is seen in the C ring and Cassini division while the low levels of aliphatic material observed by VIMS in the A and B rings particles are an evidence that they are pristine. Thermal properties: the ring-particles' temperature is retrieved by fitting the spectral position of the 3.6 mu m continuum peak observed on reflectance spectra: in case of pure water ice the position of the peak, as measured in laboratory, shifts towards shorter wavelengths when temperature decreases, moving from about 3.65 mu m at 123 K to about 3.55 mu m at 88 K. When applied to VIMS rings observations, this method allows us to infer the average temperature across ring regions sampled through 400 km-wide radial bins. Comparing VIMS temperature radial profiles with similar CIRS measurements acquired at the same time we have found a substantial agreement between the two instruments' results across the A and B rings. In general VIMS measures higher temperatures than CIRS across C ring and Cassini division as a consequence of the lower optical depth and the resulting pollution that creates a deviation from pure water ice composition of these regions. VIMS results point out that across C ring and CD the 3.6 mu m peak wavelength is always higher than across B and A rings and therefore C ring and CD are warmer than A and B rings. VIMS observations allow us to investigate also diurnal and seasonal effects: comparing antisolar and subsolar ansae observations we have measured higher temperature on the latter.
   As the solar elevation angle decreases to 0 degrees (equinox), the peak's position shifts at shorter wavelengths because ring's particles becomes colder. Merging multi-wavelength data sets allow us to test different thermal models, combining the effects of particle albedo, regolith composition, grain size and thermal properties with the ring structures. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Filacchione, G.; Ciarniello, M.; Capaccioni, F.; Cerroni, P.] Ist Astrofis & Planetol Spaziali, INAF IAPS, I-00133 Rome, Italy.
   [Clark, R. N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80228 USA.
   [Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
   [Hedman, M. M.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
   [Cuzzi, J. N.; Cruikshank, D. P.; Ore, C. M. Dalle] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Brown, R. H.] Univ Arizona, Lunar Planetary Lab, Tucson, AZ 85721 USA.
   [Altobelli, N.] ESA ESAC, Villanueva De La Canada, Spain.
   [Spilker, L. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Filacchione, G (reprint author), Ist Astrofis & Planetol Spaziali, INAF IAPS, Via Fosso Cavaliere, I-00133 Rome, Italy.
EM gianrico.filacchione@iaps.inaf.it
OI Cerroni, Priscilla/0000-0003-0239-2741; Ciarniello,
   Mauro/0000-0002-7498-5207; Capaccioni, Fabrizio/0000-0003-1631-4314;
   Filacchione, Gianrico/0000-0001-9567-0055
FU Italian Space Agency [I/015/09/0]; NASA through the Cassini project
FX The authors thank Larry W. Esposito and Cecile Ferrari for the useful
   comments which improved the quality of the paper. This research has made
   use of NASA's Astrophysics Data System and was completed thanks to the
   financial support of the Italian Space Agency (grant I/015/09/0) and
   NASA through the Cassini project.
NR 76
TC 4
Z9 4
U1 1
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 OCT
PY 2014
VL 241
BP 45
EP 65
DI 10.1016/j.icarus.2014.06.001
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR5IG
UT WOS:000343617900004
ER

PT J
AU Eke, VR
   Bartram, SA
   Lane, DA
   Smith, D
   Teodoro, LFA
AF Eke, Vincent R.
   Bartram, Sarah A.
   Lane, David A.
   Smith, David
   Teodoro, Luis F. A.
TI Lunar polar craters - Icy, rough or just sloping?
SO ICARUS
LA English
DT Article
DE Moon, surface; Radar observations; Ices
ID WATER ICE; SPATIAL-DISTRIBUTION; HYDROGEN DEPOSITS; SOUTH-POLE; COLD
   TRAPS; RADAR; MOON; SATELLITES; ARECIBO; MERCURY
AB Circular Polarisation Ratio (CPR) mosaics from Mini-SAR on Chandrayaan-1 and Mini-RF on LRO are used to study craters near to the lunar north pole. The look direction of the detectors strongly affects the appearance of the crater CPR maps. Rectifying the mosaics to account for parallax also significantly changes the CPR maps of the crater interiors. It is shown that the CPRs of crater interiors in unrectified maps are biased to larger values than crater exteriors, because of a combination of the effects of parallax and incidence angle. Using the LOLA Digital Elevation Map (DEM), the variation of CPR with angle of incidence has been studied. For fresh craters, CPR similar to 0.7 with only a weak dependence on angle of incidence or position interior or just exterior to the crater, consistent with dihedral scattering from blocky surface roughness. For anomalous craters, the CPR interior to the crater increases with both incidence angle and distance from the crater centre. Central crater CPRs are similar to those in the crater exteriors. CPR does not appear to correlate with temperature within craters. Furthermore, the anomalous polar craters have diameter-to-depth ratios that are lower than those of typical polar craters. These results strongly suggest that the high CPR values in anomalous polar craters are not providing evidence of significant volumes of water ice. Rather, anomalous craters are of intermediate age, and maintain sufficiently steep sides that sufficient regolith does not cover all rough surfaces. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Eke, Vincent R.; Bartram, Sarah A.; Lane, David A.; Smith, David] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3HP, England.
   [Teodoro, Luis F. A.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, BAER,Planetary Syst Branch, Moffett Field, CA 94035 USA.
RP Eke, VR (reprint author), Univ Durham, Dept Phys, Inst Computat Cosmol, S Rd, Durham DH1 3HP, England.
EM v.r.eke@durham.ac.uk
FU Science and Technology Facilities Council [ST/F001166/1]; LASER program;
   PGG NASA program
FX V.R.E. thanks Randy Kirk for helpful comments. We would like to thank
   the referees for their helpful comments. This work was supported by the
   Science and Technology Facilities Council [Grant No. ST/F001166/1], L.T.
   acknowledges the support of the LASER and PGG NASA programs for funding
   this research.
NR 44
TC 3
Z9 4
U1 2
U2 11
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 2014
VL 241
BP 66
EP 78
DI 10.1016/j.icarus.2014.06.021
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR5IG
UT WOS:000343617900005
ER

PT J
AU Davies, AG
   Veeder, GJ
   Hill, SI
   Matson, DL
   Johnson, TV
AF Davies, A. G.
   Veeder, G. J.
   Hill, S. I.
   Matson, D. L.
   Johnson, T. V.
TI Charting thermal emission variability at Amirani with the Galileo NIMS
   Io Thermal Emission Database (NITED)
SO ICARUS
LA English
DT Article
DE Io; Volcanism; Infrared observations; Jupiter, satellites; Satellites,
   surfaces
ID INFRARED MAPPING SPECTROMETER; JUPITERS MOON IO; VOLCANIC ACTIVITY;
   HEAT-FLOW; HOT-SPOTS; TEMPERATURE; PROMETHEUS; SIGNATURE; ERUPTIONS;
   MISSION
AB We have examined the variability of thermal emission from lava flows at Amirani on Io, using measurements of radiant flux from detections by the Galileo Near Infrared Mapping Spectrometer (NIMS) between 1996 and 2001. Amirani is the longest currently active lava flow field in the Solar System and a persistent thermal source in every Galileo NIMS observation that covers its location. We have quantified the thermal emission from hot spots correlated with discrete areas of new lava flow emplacement at points along the length of the Amirani flow field in high spatial resolution NIMS observations in 2000 and 2001. Where discernible, the position of some effusive activity changes from orbit to orbit. We find the implied style of emplacement of lava at Amirani is consistent with pahoehoe-like flows. There is an estimated 50% decrease in discharge rate between 1997 and late 2001, perhaps linked to an outburst eruption in the Amirani vicinity in February 2001. The variability of thermal emission from Amirani is less than that seen at a number of other persistently active ionian volcanoes (such as Prometheus, Culann, and Loki Patera). All of these volcanoes exhibit large increases and decreases in the absolute magnitude of thermal emission (see Matson et al., 2006 [Loki Patera]; Davies, A.G. et al. [2006]. Icarus 184, 460-477 [Prometheus]; and Davies, A.G., Ennis, M.E. [2011]. Icarus 215, 401-416 [Culann]). At Amirani, as at these volcanoes, the thermal emission measured between 1996 and 2001 indicates a persistent, although variable, supply of magma to the surface. In high spatial resolution NIMS observations of hot spots obtained in 2000 and 2001 we estimate the emitted power from active lava flows associated with Amirani to be similar to 170 +/- 30 GW, which corresponds to total effusion rates (assuming a basaltic composition) from multiple points along the Amirani flow of 34-56 m(3)/s. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Davies, A. G.; Matson, D. L.; Johnson, T. V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Veeder, G. J.] Bear Fight Inst, Winthrop, WA 98862 USA.
   [Hill, S. I.] Coulsdon Coll, Old Coulsdon CR5 1YA, England.
RP Davies, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Ms 183-401, Pasadena, CA 91109 USA.
EM Ashley.Davies@jpl.nasa.gov
FU NASA Outer Planets Research Program
FX This work was conducted at the Jet Propulsion Laboratory, California
   Institute of Technology, under contract with NASA, and is supported by
   the NASA Outer Planets Research Program. AGD especially thanks
   Jean-Philippe Combe of the Bear Fight Institute, Winthrop, WA, for
   providing ENVI-readable NIMS products. We thank Giovanni Leone and an
   anonymous reviewer for their reviews of the manuscript. (c) 2014
   Caltech. All rights reserved.
NR 44
TC 4
Z9 4
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 2014
VL 241
BP 190
EP 199
DI 10.1016/j.icarus.2014.06.034
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR5IG
UT WOS:000343617900014
ER

PT J
AU Le Gall, A
   Leyrat, C
   Janssen, MA
   Keihm, S
   Wye, LC
   West, R
   Lorenz, RD
   Tosi, F
AF Le Gall, A.
   Leyrat, C.
   Janssen, M. A.
   Keihm, S.
   Wye, L. C.
   West, R.
   Lorenz, R. D.
   Tosi, F.
TI Iapetus' near surface thermal emission modeled and constrained using
   Cassini RADAR Radiometer microwave observations
SO ICARUS
LA English
DT Article
DE Iapetus; Radar observations; Radio observations; Satellites, surfaces;
   Geological processes
ID COHERENT BACKSCATTER; 2.2-CM WAVELENGTH; DARK MATERIAL; SATELLITES;
   PHOEBE; TETHYS; DIONE; RHEA; TEMPERATURES; ENCELADUS
AB Since its arrival at Saturn, the Cassini spacecraft has had only a few opportunities to observe Iapetus, Saturn's most distant regular satellite. These observations were all made from long ranges (>100,000 km) except on September 10, 2007, during Cassini orbit 49, when the spacecraft encountered the two-toned moon during its closest flyby so far. In this pass it collected spatially resolved data on the object's leading side, mainly over the equatorial dark terrains of Cassini Regio (CR). In this paper, we examine the radiometry data acquired by the Cassini RADAR during both this close-targeted flyby (referred to as IA49-3) and the distant Iapetus observations. In the RADAR's passive mode, the receiver functions as a radiometer to record the thermal emission from planetary surfaces at a wavelength of 2.2-cm. On the cold icy surfaces of Saturn's moons, the measured brightness temperatures depend both on the microwave emissivity and the physical temperature profile below the surface down to a depth that is likely to be tens of centimeters or even a few meters. Combined with the concurrent active data, passive measurements can shed light on the composition, structure and thermal properties of planetary regoliths and thus on the processes from which they have formed and evolved. The model we propose for Iapetus' microwave thermal emission is fitted to the IA49-3 observations and reveals that the thermal inertias sensed by the Cassini Radiometer over both CR and the bright mid-to-high latitude terrains, namely Ronceveaux Terra (RT) in the North and Saragossa Terra (ST) in the South, significantly exceed those measured by Cassini's CIRS (Composite Infrared Spectrometer), which is sensitive to much smaller depths, generally the first few millimeters of the surface. This implies that the subsurface of Iapetus sensed at 2.2-cm wavelength is more consolidated than the uppermost layers of the surface. In the case of CR, a thermal inertia of at least 50 J m(-2) K-1 S-1/2, and most probably >200 J m(-2) K-1 S-1/2 is inferred. This suggests a gradient in density with depth or, more likely, that the Radiometer has probed the icy substrate underlying the dark layer. Furthermore, the measured thermal emission is found to arise from the upper few meters of the subsurface, which points to tholins, rather than iron oxide compounds, as the primary contaminants of the dark material. We also find that, although there is a latitudinal decrease probably related to the thinning of the dark layer away from the Equator, the CR region exhibits a high 2.2-cm emissivity, 0.87 in average, which is close to the emissivity of Phoebe, a putative source of the dark matter. In the case of RT + ST, model fitting points to a mean thermal inertia of 160 J m(-2) K-1 S-1/2 along with the possible presence of an absorbing compound in the regolith of the bright terrains. Nevertheless, this layer is transparent enough for the Radiometer to capture the seasonal contrast between the northern and southern hemispheres. Lastly, a global decline of the microwave emissivity with latitude is revealed; it is probably indicative of a progressive increase of the water ice content in the near surface. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Le Gall, A.] UVSQ, IPSL, Lab Atmospheres Milieux Observat Spatials LATMOS, F-78280 Guyancourt, France.
   [Leyrat, C.] Observ Paris, LESIA, F-92195 Meudon, France.
   [Janssen, M. A.; Keihm, S.; West, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Wye, L. C.] SRI Int, Menlo Pk, CA 94025 USA.
   [Lorenz, R. D.] Johns Hopkins Univ, Dept Space, Appl Phys Lab, Planetary Explorat Grp, Laurel, MD 20723 USA.
   [Tosi, F.] Ist Nazl Astrofis, Inst Astrofis & Planetol Spaziali, I-00133 Rome, Italy.
RP Le Gall, A (reprint author), UVSQ, IPSL, Lab Atmospheres Milieux Observat Spatials LATMOS, 11 Bd Alembert, F-78280 Guyancourt, France.
EM Alice.Legall@latmos.ipsl.fr
RI Lorenz, Ralph/B-8759-2016; 
OI Lorenz, Ralph/0000-0001-8528-4644; Tosi, Federico/0000-0003-4002-2434
FU NASA Postdoctoral Program; NASA
FX The authors wish to thank the Cassini-Huygens team for the design,
   development, and operation of the mission. The Cassini-Huygens mission
   is a joint endeavor of NASA, the European Space Agency (ESA), and the
   Italian Space Agency (ASI) and is managed by JPL/Caltech under a
   contract with NASA. The authors also wish to acknowledge the key role
   played by Steve Ostro in the planning and design of the Cassini RADAR
   observations of Iapetus. This paper is dedicated to him. The authors are
   grateful to David Blackburn for providing us with the map of Iapetus'
   Bond albedo (published in Blackburn et al., 2011). Part of this work has
   been conducted at the Jet Propulsion Laboratory, California Institute of
   Technology; A. Le Gall was then supported by the NASA Postdoctoral
   Program, administrated by Oak Ridge Associated Universities (ORAU). She
   now benefits from a Chair of the French Space Agency CNES/UVSQ
   (Universite Versailles Saint-Quentin).
NR 67
TC 4
Z9 4
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 OCT
PY 2014
VL 241
BP 221
EP 238
DI 10.1016/j.icarus.2014.06.011
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR5IG
UT WOS:000343617900016
ER

PT J
AU Howett, CJA
   Spencer, JR
   Hurford, T
   Verbiscer, A
   Segura, M
AF Howett, C. J. A.
   Spencer, J. R.
   Hurford, T.
   Verbiscer, A.
   Segura, M.
TI Thermophysical property variations across Dione and Rhea
SO ICARUS
LA English
DT Article
DE Saturn, satellites; Ices; Infrared observations; Satellites, surfaces
ID THERMAL INERTIA; SATURN SYSTEM; CASSINI VIMS; E-RING; ENCELADUS; ORIGIN;
   SPECTROMETER; ATMOSPHERE; HISTORY; TETHYS
AB Maps of the variation in bolometric Bond albedo and thermal inertia across Rhea and Dione have been produced using various day and nighttime observations, taken by Cassini's Composite Infrared Spectrometer (CIRS). The albedo maps show the same trend that has been previously observed on these satellites from reflected sunlight and thermal observations: a higher albedo on their leading hemispheres. The thermal inertia maps show two previously unknown anomalous high thermal inertia regions: low latitudes on Dione's leading hemisphere and the bright ejecta blanket of Rhea's Inktomi crater.
   The thermal inertia on Diane increases modestly from a background value of 8 J m(-2) K-1 s(-1/2) to 11 J m(-2) K-1 s(-1/2) in a region preferentially bombarded by high-energy electrons. We believe that this region on Diane is probably analogous to the thermally anomalous regions recently discovered at equivalent locations on Mimas and Tethys, dubbed Pac-Man features. The smaller magnitude of Dione's thermal anomaly, compared to that of Mimas and Tethys, provides additional evidence that surface alteration by high-energy electrons produces these anomalies, as the high-energy electron flux decreases with increasing distance from Saturn. However, unlike on Mimas and Tethys, the thermally anomalous region on Dione does not display a spatially correlated decrease in the IR/UV (0.930 mu m/0.338 mu m) color ratio, implying that the minimum electron energy threshold of the IR/UV ice surface darkening mechanism is not met on Dione. The average of the mapped bolometric Bond albedos on the leading and trailing hemispheres of Diane are 0.49 +/- 0.11 and 0.44 +/- 0.13 respectively.
   On Rhea the thermal inertia increases from a background value of 10 J m(-2) K-1 s(-1/2) to 19 J m(-2) K-1 s(-1/2) on the ejecta blanket of Inktomi crater, probably due to a mixture of high and low thermal inertia material in this region, such as a fine- and large-grain ice mixture. This is the first time a thermal inertia anomaly has been associated with an impact crater on an icy saturnian satellite. On Rhea the average of the mapped bolometric Bond albedos on the leading and trailing hemispheres are 0.59 +/- 0.11 and 0.56 +/- 0.13 respectively. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Howett, C. J. A.; Spencer, J. R.; Segura, M.] Southwest Res Inst, Boulder, CO 80302 USA.
   [Hurford, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Verbiscer, A.] Univ Virginia, Charlottesville, VA 22904 USA.
RP Howett, CJA (reprint author), 1050 Walnut St,Suite 300, Boulder, CO 80302 USA.
EM howett@boulder.swri.edu
RI Hurford, Terry/F-2625-2012
FU NASA Cassini Data Analysis program [NNX12AC23G]
FX Thanks is given to the NASA Cassini Data Analysis program, which funded
   this work (NNX12AC23G), to Dr. C. Paranicas for supplying the electron
   power contours shown in Figs. 1 and 4 and to the Cassini Project.
NR 39
TC 7
Z9 7
U1 1
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 2014
VL 241
BP 239
EP 247
DI 10.1016/j.icarus.2014.05.047
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR5IG
UT WOS:000343617900017
ER

PT J
AU El-Maarry, MR
   Watters, W
   McKeown, NK
   Carter, J
   Dobrea, EN
   Bishop, JL
   Pommerol, A
   Thomas, N
AF El-Maarry, M. R.
   Watters, W.
   McKeown, N. K.
   Carter, J.
   Dobrea, E. Noe
   Bishop, J. L.
   Pommerol, A.
   Thomas, N.
TI Potential desiccation cracks on Mars: A synthesis from modeling,
   analogue-field studies, and global observations
SO ICARUS
LA English
DT Article
DE Mars; Mars, surface; Geological processes; Mars, climate
ID CLAY MINERAL FORMATION; OMEGA/MARS EXPRESS; MERIDIANI-PLANUM; MAWRTH
   VALLIS; SOUTHERN HIGHLANDS; POLYGONAL CRACKS; GEOLOGIC RECORD; NORTHERN
   PLAINS; BURNS FORMATION; THARSIS REGION
AB Potential desiccation polygons (PDPs) are polygonal surface patterns that are a common feature in Noa-chian-to-Hesperian-aged phyllosilicate- and chloride-bearing terrains and have been observed with size scales that range from cm-wide (by current rovers) to 10s of meters-wide. The global distribution of PDPs shows that they share certain traits in terms of morphology and geologic setting that can aid identification and distinction from fracturing patterns caused by other processes. They are mostly associated with sedimentary deposits that display spectral evidence for the presence of Fe/Mg smectites, Al-rich smectites or less commonly kaolinites, carbonates, and sulfates. In addition, PDPs may indicate paleolacustrine environments, which are of high interest for planetary exploration, and their presence implies that the fractured units are rich in smectite minerals that may have been deposited in a standing body of water. A collective synthesis with new data, particularly from the HiRISE camera suggests that desiccation cracks may be more common on the surface of Mars than previously thought. A review of terrestrial research on desiccation processes with emphasis on the theoretical background, field studies, and modeling constraints is presented here as well and shown to be consistent with and relevant to certain polygonal patterns on Mars. (C) 2014 Elsevier Inc. All rights reserved.
C1 [El-Maarry, M. R.; Pommerol, A.; Thomas, N.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
   [Watters, W.] Wellesley Coll, Dept Astron, Whitin Observ, Wellesley, MA 02481 USA.
   [McKeown, N. K.] MacEwan Univ, Dept Phys Sci, Edmonton, AB, Canada.
   [Carter, J.] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France.
   [Dobrea, E. Noe] Planetary Sci Inst, Tucson, AZ 85719 USA.
   [Dobrea, E. Noe] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Bishop, J. L.] SETI Inst, Mountain View, CA 94043 USA.
RP El-Maarry, MR (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland.
EM mohamed.elmaarry@space.unibe.ch
OI EL-MAARRY, MOHAMED RAMY/0000-0002-8262-0320
FU Swiss National Science Foundation (SNSF); NASA; Mars Data Analysis
   Program (MDAP)
FX M.R.El-M. would like to thank the numerous co-authors, mentors and
   colleagues that have directly and indirectly contributed immensely to
   this project over the years as well as previously published studies.
   M.R.El-M., A.P. and N.T. are supported by funding from the Swiss
   National Science Foundation (SNSF). W.W. would like to thank NASA for
   the continued funding. E.N-D. is funded by the Mars Data Analysis
   Program (MDAP). The authors would like to thank Marjorie Chan and an
   anonymous reviewer for their helpful reviews that have considerably
   improved the paper.
NR 159
TC 10
Z9 10
U1 1
U2 11
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD OCT
PY 2014
VL 241
BP 248
EP 268
DI 10.1016/j.icarus.2014.06.033
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR5IG
UT WOS:000343617900018
ER

PT J
AU Charnay, B
   Forget, F
   Tobie, G
   Sotin, C
   Wordsworth, R
AF Charnay, Benjamin
   Forget, Francois
   Tobie, Gabriel
   Sotin, Christophe
   Wordsworth, Robin
TI Titan's past and future: 3D modeling of a pure nitrogen atmosphere and
   geological implications
SO ICARUS
LA English
DT Article
DE Titan, atmosphere; Titan, hydrology; Atmospheres, evolution
ID SATURNS MOON TITAN; SURFACE TEMPERATURES; METHANE CYCLE; ORIGIN;
   EVOLUTION; CLIMATE; CLOUDS; LAKES; CONVECTION; SCATTERING
AB Several clues indicate that Titan's atmosphere has been depleted in methane during some period of its history, possibly as recently as 0.5-1 billion years ago. It could also happen in the future. Under these conditions, the atmosphere becomes only composed of nitrogen with a range of temperature and pressure allowing liquid or solid nitrogen to condense. Here, we explore these exotic climates throughout Titan's history with a 3D Global Climate Model (GCM) including the nitrogen cycle and the radiative effect of nitrogen clouds. We show that for the last billion years, only small polar nitrogen lakes should have formed. Yet, before 1 Ga, a significant part of the atmosphere could have condensed, forming deep nitrogen polar seas, which could have flowed and flooded the equatorial regions. Alternatively, nitrogen could be frozen on the surface like on Triton, but this would require an initial surface albedo higher than 0.65 at 4 Ga. Such a state could be stable even today if nitrogen ice albedo is higher than this value. According to our model, nitrogen flows and rain may have been efficient to erode the surface. Thus, we can speculate that a paleo-nitrogen cycle may explain the erosion and the age of Titan's surface, and may have produced some of the present valley networks and shorelines. Moreover, by diffusion of liquid nitrogen in the crust, a paleo-nitrogen cycle could be responsible of the flattening of the polar regions and be at the origin of the methane outgassing on Titan. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Charnay, Benjamin; Forget, Francois] Univ Paris 06, CNRS, Lab Meteorol Dynam, Paris, France.
   [Charnay, Benjamin] Univ Washington, Virtual Planetary Lab, Seattle, WA 98195 USA.
   [Tobie, Gabriel] Univ Nantes, Lab Planetol & Geodynam, UMR CNRS 6112, Nantes, France.
   [Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Wordsworth, Robin] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
RP Charnay, B (reprint author), Univ Paris 06, CNRS, Lab Meteorol Dynam, Paris, France.
EM bclmd@lmd.jussieufr
FU NASA Astrobiology Institute program
FX C.S. acknowledges support by the NASA Astrobiology Institute program.
NR 58
TC 3
Z9 3
U1 8
U2 24
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 2014
VL 241
BP 269
EP 279
DI 10.1016/j.icarus.2014.07.009
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR5IG
UT WOS:000343617900019
ER

PT J
AU D'Angelo, G
   Weidenschilling, SJ
   Lissauer, JJ
   Bodenheimer, P
AF D'Angelo, Gennaro
   Weidenschilling, Stuart J.
   Lissauer, Jack J.
   Bodenheimer, Peter
TI Growth of Jupiter: Enhancement of core accretion by a voluminous
   low-mass envelope
SO ICARUS
LA English
DT Article
DE Accretion; Jovian planets; Jupiter; Planetary formation; Planetesimals
ID GIANT PLANET FORMATION; NEBULAR GAS DRAG; SOLAR NEBULA; PROTOPLANETARY
   ATMOSPHERES; COLLISIONAL FRAGMENTATION; PEBBLE ACCRETION; GALILEO PROBE;
   PLANETESIMALS; MODELS; SIMULATIONS
AB We present calculations of the early stages of the formation of Jupiter via core nucleated accretion and gas capture. The core begins as a seed body of about 350 km in radius and orbits in a swarm of planetesimals whose initial radii range from 15 m to 50 km. The evolution of the swarm accounts for growth and fragmentation, viscous and gravitational stirring, and for drag-assisted migration and velocity damping. During this evolution, less than 9% of the mass is in planetesimals smaller than 1 km in radius; less than or similar to 25% is in planetesimals with radii between 1 and 10 km; and less than or similar to 7% is in bodies with radii larger than 100 km. Gas capture by the core substantially enhances the size-dependent cross-section of the planet for accretion of planetesimals. The calculation of dust opacity in the planet's envelope accounts for coagulation and sedimentation of dust particles released as planetesimals are ablated. The calculation is carried out at an orbital semi-major axis of 5.2 AU and the initial solids' surface density is 10 g cm(-2) at that distance. The results give a core mass of nearly 7.3 Earth masses (M-circle plus) and an envelope mass of approximate to 0.15 M-circle plus after about 4 x 10(5) years, at which point the envelope growth rate surpasses that of the core. The same calculation without the envelope yields a core of only about 4.4 M-circle plus. (C) 2014 Elsevier Inc. All rights reserved.
C1 [D'Angelo, Gennaro; Lissauer, Jack J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
   [D'Angelo, Gennaro] SETI Inst, Mountain View, CA 94043 USA.
   [Weidenschilling, Stuart J.] Planetary Sci Inst, Tucson, AZ 85719 USA.
   [Bodenheimer, Peter] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
RP D'Angelo, G (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA.
EM gennaro.dangelo@nasa.gov
OI D'Angelo, Gennaro/0000-0002-2064-0801
FU NASA Outer Planets Research Program [202844.02.02.01.75]
FX This project was funded by NASA Outer Planets Research Program Grant
   202844.02.02.01.75. We are grateful to Olenka Hubickyj for helpful
   discussions and useful feedback on this work, and to two anonymous
   referees whose comments and suggestions helped improve this paper. G.D.
   thanks Los Alamos National Laboratory for its hospitality. Resources
   supporting this study were provided by the NASA High-End Computing (HEC)
   Program through the NASA Advanced Supercomputing (NAS) Division at Ames
   Research Center and the NASA Center for Climate Simulation (NCCS) at
   Goddard Space Flight Center.
NR 67
TC 4
Z9 4
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 2014
VL 241
BP 298
EP 312
DI 10.1016/j.icarus.2014.06.029
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR5IG
UT WOS:000343617900021
ER

PT J
AU Lavvas, P
   West, RA
   Gronoff, G
   Rannou, P
AF Lavvas, P.
   West, R. A.
   Gronoff, G.
   Rannou, P.
TI Titan's emission processes during eclipse
SO ICARUS
LA English
DT Article
DE Titan; Eclipses; Aurorae
ID UPPER-ATMOSPHERE; COSMIC-RAYS; PHOTOCHEMISTRY; HYDROCARBONS;
   FLUORESCENCE; IONOSPHERE; IONIZATION; AEROSOLS; SURFACE; MODEL
AB Observations of Titan's emissions during its 2009 eclipse by Saturn revealed a weak airglow around the moon, as well as a brighter emission from its disk (West et al. [2012]. Geophys. Res. Lett. 39 (1), 18204). We explore here the potential mechanisms that could generate these emissions and more specifically the role of magnetospheric plasma and cosmic rays in the upper and lower atmosphere, respectively. We consider excitation of N-2 by these energy sources and calculate the resulting emissions through a detailed model of N-2 airglow followed by careful radiation transfer of the emitted photons through the atmosphere, and into the UVIS and ISS instruments. Our results indicate that the observed limb emissions are consistent with magnetospheric plasma energy input, while emissions instigated by cosmic ray excitation are very weak and cannot explain the observed disk emissions. We discuss possible contributions from other sources that could potentially explain the disk observations. The most likely scenario is that of scattered stellar light from Titan's disk. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Lavvas, P.; Rannou, P.] Univ Reims, GSMA UMR 7331, F-51687 Reims, France.
   [West, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Gronoff, G.] NASA, SSAI LaRC, Chem & Dynam Branch, Sci Directorate, Hampton, VA 23681 USA.
RP Lavvas, P (reprint author), Univ Reims, GSMA UMR 7331, F-51687 Reims, France.
EM panayotis.lavvas@univ-reims.fr
RI RANNOU, Pascal/I-9059-2012; 
OI Gronoff, Guillaume/0000-0002-0331-7076
FU Universite de Reims; French space agency (CNES); Cassini project; French
   organization CNRS; National Astrobiology Institute
FX We acknowledge fruitful input from discussions with Roger Yelle and the
   Cassini/UVIS team. We thank Erich Karkoschka for supplying a table of
   methane absorption coefficients and Caitlin Griffith for providing
   tables of Legendre polynomial coefficients for the aerosol phase
   functions tabulated by Tomasko et al. (2008). R. West was supported by
   the Universite de Reims and by the French organization CNRS. P. Lavvas
   was supported by the French space agency (CNES) as a Cassini
   Participating Scientist. Part of this work was done by the Jet
   Propulsion Laboratory, California Institute of Technology, supported by
   the Cassini project and by the National Astrobiology Institute.
NR 40
TC 4
Z9 4
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 OCT
PY 2014
VL 241
BP 397
EP 408
DI 10.1016/j.icarus.2014.07.008
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AR5IG
UT WOS:000343617900028
ER

PT J
AU Siochi, EJ
AF Siochi, Emilie J.
TI Graphene in the sky and beyond
SO NATURE NANOTECHNOLOGY
LA English
DT Editorial Material
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Siochi, EJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM emilie.j.siochi@nasa.gov
NR 9
TC 8
Z9 8
U1 1
U2 22
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1748-3387
EI 1748-3395
J9 NAT NANOTECHNOL
JI Nat. Nanotechnol.
PD OCT
PY 2014
VL 9
IS 10
BP 745
EP 747
PG 3
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA AR5IA
UT WOS:000343617200011
PM 25286266
ER

PT J
AU Zhang, QY
   Cheng, YB
   Lyapustin, AI
   Wang, YJ
   Gao, F
   Suyker, A
   Verma, S
   Middleton, EM
AF Zhang, Qingyuan
   Cheng, Yen-Ben
   Lyapustin, Alexei I.
   Wang, Yujie
   Gao, Feng
   Suyker, Andrew
   Verma, Shashi
   Middleton, Elizabeth M.
TI Estimation of crop gross primary production (GPP): fAPAR(chl) versus
   MOD15A2 FPAR
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE GPP; MODIS; MOD15A2 FPAR; fAPARchl
ID LEAF-AREA INDEX; LIGHT-USE EFFICIENCY; FOREST ECOSYSTEM PROCESSES;
   REMOTE ESTIMATION; WATER-CONTENT; CHLOROPHYLL FAPAR(CHL); REGIONAL
   APPLICATIONS; CANOPY REFLECTANCE; TEMPERATE FOREST; GENERAL-MODEL
AB Photosynthesis (PSN) is a pigment level process in which antenna pigments (predominately chlorophylls) in chloroplasts absorb photosynthetically active radiation (PAR) for the photochemical process. PAR absorbed by foliar non-photosynthetic components is not used for PSN. The fraction of PAR absorbed (fAPAR) by a canopy/vegetation (i.e., fAPAR(canopy)) derived from the Moderate Resolution Imaging Spectroradiometer (MODIS) images, referred to as MOD15A2 FPAR, has been used to compute absorbed PAR (APAR) for PSN (APAR(PSN)) which is utilized to produce the standard MODIS gross primary production (GPP) product, referred to as MOD17A2 GPP. In this study, the fraction of PAR absorbed by chlorophyll throughout the canopy (fAPAR(chl)) was retrieved from MODIS images for three AmeriFlux crop fields in Nebraska. There are few studies in the literature that compare the performance of MOD15A2 FPAR versus fAPAR(chl) in GPP estimation. In our study MOD15A2 FPAR and the retrieved fAPAR(chl) were compared with field fAPAR(canopy) and the fraction of PAR absorbed by green leaves of the vegetation (fAPAR(green)). MOD15A2 FPAR overestimated field fAPAR(canopy) in spring and in fall, and underestimated field fAPAR(canopy) in midsummer whereas fAPAR(chl) correctly captured the seasonal phenology. The retrieved fAPAR(chl) agreed well with field fAPAR(green) at early crop growth stage in June, and was less than field fAPAR(green) in late July, August and September. GPP estimates with fAPAR(chl) and with MOD15A2 FPAR were compared to tower flux GPP. GPP simulated with fAPAR(chl) was corroborated with tower flux GPP. Improvements in crop GPP estimation were achieved by replacing MOD15A2 FPAR with fAPAR(chl) which also reduced uncertainties of crop GPP estimates by 1.12-237 g C m(-2) d(-1). (C) 2014 Elsevier Inc. All rights reserved.
C1 [Zhang, Qingyuan] Univ Space Res Assoc, Columbia, MD 21044 USA.
   [Zhang, Qingyuan; Cheng, Yen-Ben; Wang, Yujie; Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
   [Cheng, Yen-Ben] Sigma Space Corp, Lanham, MD 20706 USA.
   [Lyapustin, Alexei I.] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA.
   [Wang, Yujie] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
   [Gao, Feng] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA.
   [Suyker, Andrew; Verma, Shashi] Univ Nebraska, Sch Nat Resources, Lincoln, NE 68588 USA.
RP Zhang, QY (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Bldg 33,Room G321,Code 618, Greenbelt, MD 20771 USA.
EM qyz72@yahoo.com
FU NASA Terrestrial Ecology project [NNX12AJ51G]; NASA Science of Terra and
   Aqua project [NNX14AK50G]; Carbon Dioxide Information Analysis Center at
   the Oak Ridge National Laboratory of the Department of Energy
FX This study was supported by NASA Terrestrial Ecology project (Grant No.,
   NNX12AJ51G; PI, Q. Zhang) and NASA Science of Terra and Aqua project
   (Grant No., NNX14AK50G; PI, Q. Zhang) (Dr. Diane Wickland, manager). We
   would like to thank the support and the use of facilities and equipment
   provided by the Center for Advanced Land Management Information
   Technologies and the Carbon Sequestration program, University of
   Nebraska Lincoln. Site-specific climate and CO<INF>2</INF> flux data are
   distributed by AmeriFlux network (http://public.ornl.gov/ameriflux),
   supported by Carbon Dioxide Information Analysis Center at the Oak Ridge
   National Laboratory of the Department of Energy. We are grateful to Drs.
   Anatoly Gitelson and Yi Peng for helpful discussion and comments and for
   providing field fAPAR<INF>canopy</INF>, fAPAR<INF>green</INF>, LAI and
   LAI<INF>green</INF>. USDA is an equal opportunity provider and employer.
NR 50
TC 12
Z9 12
U1 5
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 2014
VL 153
BP 1
EP 6
DI 10.1016/j.rse.2014.07.012
PG 6
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
   Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
   Photographic Technology
GA AR5KI
UT WOS:000343623300001
ER

PT J
AU Gross, J
   Isaacson, PJ
   Treiman, AH
   Le, L
   Gorman, JK
AF Gross, Juliane
   Isaacson, Peter J.
   Treiman, Allan H.
   Le, Loan
   Gorman, Julia K.
TI Spinel-rich lithologies in the lunar highland crust: Linking lunar
   samples with crystallization experiments and remote sensing
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Lunar; pink spinel; M-3; V/NIR reflectance spectra; crystallization
   experiments; spinel-rich lithologies; remote sensing; Apollo 65875
ID IMPACT MELT; MOON; TROCTOLITE; ASSIMILATION; ANORTHOSITE; DISSOLUTION;
   METEORITES; PERIDOTITE; MINERALOGY; ANORTHITE
AB Mg-Al spinel is rare in lunar rocks (Apollo and meteorite collections), and occurs mostly in troctolites and troctolitic cataclastites. Recently, a new lunar lithology, rich in spinel and plagioclase, and lacking abundant olivine and pyroxene, was recognized in visible to near-infrared (VNIR) reflectance spectra by the Moon Mineralogy Mapper (M-3) instrument on the Chandrayaan-1 spacecraft at the Moscoviense basin. These outcrop-scale areas are inferred to contain 20-30% Mg-Al spinel. Possible explanations for the petrogenesis of spinel-bearing and spinel-rich lithology(s) range from low-pressure near-surface crystallization to a deep-seated origin in the lower lunar crust or upper mantle. Here, we describe 1-bar crystallization experiments conducted on rock compositions rich in olivine and plagioclase that crystallize spinel. This would be equivalent to impact-melting, which is moderately common among lunar plutonic rocks and granulites. To explore possible precursor materials and the maximum amount of spinel that could be crystallized, a lunar troctolitic composition similar to Apollo pink spinel troctolite 65785, and a composition similar to ALHA81005 as analog to the source region of this meteorite have been chosen. The crystallization experiments on the composition of AHLA 81005 did not yield any spinel; experiments on the composition similar to Apollo 65785 crystallized a maximum of similar to 8 wt% spinel, much less than the suggested 20-30% spinel of the new lithology detected by M-3. However, our VNIR spectral reflectance analyses of the experimental run products indicate that the spinel composition of the experimental run products not only appears to be similar to the composition of the spinel lithology detected by M-3 (characteristics of the spinel absorption), but also that the modal abundances of coexisting phases (e.g., mafic glass) influence the spectral reflectance properties. Thus, the spinel-rich deposits detected by M-3 might not be as spinel-rich as previously thought and could contain as little as 4-5 wt% spinel. However, the effect of space weathering on spinel is unknown and could significantly weaken its 2 mu m absorptions. If this occurs, weathered lunar rocks could contain more spinel than a comparison with our unweathered experimental charges would suggest.
C1 [Gross, Juliane] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA.
   [Isaacson, Peter J.] Hawaii Inst Geophys & Planetol, SOEST, Honolulu, HI 96822 USA.
   [Treiman, Allan H.; Gorman, Julia K.] Lunar & Planetary Inst, Houston, TX 77058 USA.
   [Le, Loan] NASA, Jacobs Technol, JETS, Johnson Space Ctr Engn Technol & Sci, Houston, TX 77058 USA.
RP Gross, J (reprint author), Amer Museum Nat Hist, Dept Earth & Planetary Sci, Cent Pk West & 79th St, New York, NY 10024 USA.
EM jgross@amnh.org
FU NASA COS Grant [NNX13AF54G]
FX We are grateful to A. Peslier for assistance with the EMP analyses at
   NASA JSC. We thank Justin Filiberto for very helpful and fruitful
   discussions. We thank C. Pieters, S. Parman, and T. Prissel for helpful
   reviews and comments of this manuscript as well as R. Klima for handling
   this manuscript and extremely helpful thoughts and comments. Supported
   by NASA COS Grant NNX13AF54G to J. Gross; LPI contribution #1802.
NR 63
TC 4
Z9 5
U1 0
U2 5
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 2014
VL 99
IS 10
BP 1849
EP 1859
DI 10.2138/am-2014-4780
PG 11
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA AQ6XH
UT WOS:000342956700006
ER

PT J
AU Xu, HF
   Shen, ZZ
   Konishi, H
   Luo, GF
AF Xu, Huifang
   Shen, Zhizhang
   Konishi, Hiromi
   Luo, Gufeng
TI Crystal structure of Guinier-Preston zones in orthopyroxene: Z-contrast
   imaging and ab inito study
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Orthopyroxene; diopside; GP zone; nanomineral; DFT; Z-contrast imaging;
   order-disorder; enstatite
ID TERRESTRIAL ORTHO-PYROXENE; METEORITIC ORTHO-PYROXENE; SPACE GROUP
   P21CA; ORDER-DISORDER; HIGH-TEMPERATURE; LUNAR; KINETICS;
   ORTHOPYROXENES; EXSOLUTION; STABILITY
AB Nano-precipitates of Guinier-Preston zones (or G.P. zones) occur in slowly cooled orthopyroxenes (OPX). Due to their nanometer sizes and intergrowth with host OPX, both X-ray diffraction and high-resolution TEM imaging cannot provide a consistent structure model for the G.P. zone precipitates. Combining Z-contrast imaging and density functional theory (DFT) methods, a correct crystal structure for the G.P. zone precipitates can be obtained, because Z-contrast imaging can reveal positions and occupancies of atoms directly. The crystal structure for the G.P. zone has P2(1)/c symmetry with 4 types of tetrahedral chains (OA1, OA2, OB, OC). The structure can be considered as periodic stacking of half unit cells of enstatite sub-layers and of diopside sub-layers in a twinning-like relationship along a-axis. The G.P. zones that precipitate out from their host Ca-bearing OPX at low temperature are metastable with respect to end-members of enstatite and diopside.
C1 [Xu, Huifang; Shen, Zhizhang; Konishi, Hiromi] Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA.
   [Xu, Huifang] Univ Wisconsin, Mat Sci Program, Madison, WI 53706 USA.
   [Luo, Gufeng] Nanjing Univ, Dept Geosci, Nanjing 210008, Jiangsu, Peoples R China.
RP Xu, HF (reprint author), Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA.
EM hfxu@geology.wisc.edu
FU NSF [EAR-095800, EAR-0810150, DMR-0619368]; NASA Astrobiology Institute
   [N07-5489]
FX This work is supported by NSF (EAR-095800, EAR-0810150, and DMR-0619368,
   MRI) and NASA Astrobiology Institute (N07-5489). The authors thank
   Izabela Szlufarska of University of Wisconsin for the help in DFT
   calculation. The authors also thank Jun Wu and an anonymous reviewer for
   critical reviews and helpful suggestions.
NR 29
TC 2
Z9 2
U1 3
U2 12
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD OCT
PY 2014
VL 99
IS 10
BP 2043
EP 2048
DI 10.2138/am-2014-4898
PG 6
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA AQ6XH
UT WOS:000342956700023
ER

PT J
AU Derecho, I
   McCoy, KB
   Vaishampayan, P
   Venkateswaran, K
   Mogul, R
AF Derecho, I.
   McCoy, K. B.
   Vaishampayan, P.
   Venkateswaran, K.
   Mogul, R.
TI Characterization of Hydrogen Peroxide-Resistant Acinetobacter Species
   Isolated during the Mars Phoenix Spacecraft Assembly
SO ASTROBIOLOGY
LA English
DT Article
ID DEINOCOCCUS-RADIODURANS; ODYSSEY SPACECRAFT; OXIDATIVE STRESS;
   BACILLUS-PUMILUS; MICROBIAL CHARACTERIZATION; PLANETARY PROTECTION;
   CATALASE ACTIVITY; CLEAN ROOMS; RADIATION; PROTEOME
AB The microbiological inventory of spacecraft and the associated assembly facility surfaces represent the primary pool of forward contaminants that may impact the integrity of life-detection missions. Herein, we report on the characterization of several strains of hydrogen peroxide-resistant Acinetobacter, which were isolated during the Mars Phoenix lander assembly. All Phoenix-associated Acinetobacter strains possessed very high catalase specific activities, and the specific strain, A. gyllenbergii 2P01AA, displayed a survival against hydrogen peroxide (no loss in 100 mM H2O2 for 1 h) that is perhaps the highest known among Gram-negative and non-spore-forming bacteria. Proteomic characterizations reveal a survival mechanism inclusive of proteins coupled to peroxide degradation (catalase and alkyl hydroperoxide reductase), energy/redox management (dihydrolipoamide dehydrogenase), protein synthesis/folding (EF-G, EF-Ts, peptidyl-tRNA hydrolase, DnaK), membrane functions (OmpA-like protein and ABC transporter-related protein), and nucleotide metabolism (HIT family hydrolase). Together, these survivability and biochemical parameters support the hypothesis that oxidative tolerance and the related biochemical features are the measurable phenotypes or outcomes for microbial survival in the spacecraft assembly facilities, where the low-humidity (desiccation) and clean (low-nutrient) conditions may serve as selective pressures. Hence, the spacecraft-associated Acinetobacter, due to the conferred oxidative tolerances, may ultimately hinder efforts to reduce spacecraft bioburden when using chemical sterilants, thus suggesting that non-spore-forming bacteria may need to be included in the bioburden accounting for future life-detection missions. Key Words: Extremophiles-Planetary protection-Spacecraft assembly facility-Stress proteins-Microbe. Astrobiology 14, 837-847.
C1 [Derecho, I.; McCoy, K. B.; Mogul, R.] Calif State Polytech Univ Pomona, Pomona, CA 91768 USA.
   [Vaishampayan, P.; Venkateswaran, K.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Mogul, R (reprint author), Calif State Polytech Univ Pomona, Dept Chem & Biochem, 3801 W Temple Ave, Pomona, CA 91768 USA.
EM rmogul@csupomona.edu
FU NASA Astrobiology Institute; NASA Research Announcement (NRA) ROSES;
   National Aeronautics and Space Administration
FX This work was funded by the NASA Astrobiology Institute Minority
   Institutional Research Support award to R. Mogul, and in part by a NASA
   Research Announcement (NRA) ROSES 2006 award to K. Venkateswaran. A
   component of the research described in this publication was carried out
   at the Jet Propulsion Laboratory, California Institute of Technology,
   under a contract with the National Aeronautics and Space Administration.
NR 57
TC 7
Z9 7
U1 1
U2 29
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 OCT 1
PY 2014
VL 14
IS 10
BP 837
EP 847
DI 10.1089/ast.2014.1193
PG 11
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
   Geology
GA AR0AU
UT WOS:000343225700001
PM 25243569
ER

PT J
AU Taylor, PT
   Kis, KI
   Wittmann, G
AF Taylor, P. T.
   Kis, K. I.
   Wittmann, G.
TI Satellite-altitude horizontal magnetic gradient anomalies used to define
   the Kursk Magnetic Anomaly
SO JOURNAL OF APPLIED GEOPHYSICS
LA English
DT Article
DE Kursk Magnetic Anomaly; CHAMP; Swarm; Magnetic anomaly gradient
ID BANDED IRON-FORMATIONS; PANNONIAN BASIN; CHAMP SATELLITE;
   GEOMAGNETIC-FIELD; REGION
AB The Kursk Magnetic Anomaly (KMA), Russia, is one of the world's largest magnetic anomalies. We used satellite altitude horizontal gradient magnetic anomaly data to study this feature. There are two main objectives of our research; the first, to determine if the technique of the horizontal magnetic anomaly gradient analysis can be applied to CHAMP satellite altitude data to define the outline of the source of the Kursk Magnetic Anomaly (KMA). Another objective is to use the ten years of CHAMP data to reproduce the horizontal magnetic anomaly gradient data that will be measured by the two lower orbiting ESA/Swarm mission. We will be able to evaluate the application of these newer satellite altitude data for studying large areas with significant crustal magnetization. While we have acquired sufficient CHAMP orbital data to compute a horizontal gradient anomaly map from these ten years of data; the future ESA/Swarm mission will, however, allow us to compute directly the horizontal magnetic anomaly without orbital altitude and/or magnetic secular variations; however the east-west gradient that the Swarm is measuring will minimize, but not eliminate, the difference in external fields between the two lower satellites. One will still need to use relatively quiet data (e.g., K-p < 1) for crustal field mapping. Our results, developed from interpreting the satellite horizontal magnetic anomaly data, indicate that the source of the KMA is bowl shaped body open to the northwest covering an area of approximately 190,000 km(2). Published by Elsevier B.V.
C1 [Taylor, P. T.] NASA GSFC, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
   [Kis, K. I.] Eotvos Lorand Univ, Geophys & Space Sci Dept, H-1117 Budapest, Hungary.
   [Wittmann, G.] MOL Hungarian Oil & Gas Co, H-1117 Budapest, Hungary.
RP Taylor, PT (reprint author), NASA GSFC, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
EM patrick.t.taylor@nasa.gov
NR 34
TC 1
Z9 1
U1 0
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0926-9851
EI 1879-1859
J9 J APPL GEOPHYS
JI J. Appl. Geophys.
PD OCT
PY 2014
VL 109
BP 133
EP 139
DI 10.1016/j.jappgeo.2014.07.018
PG 7
WC Geosciences, Multidisciplinary; Mining & Mineral Processing
SC Geology; Mining & Mineral Processing
GA AR1II
UT WOS:000343338500013
ER

PT J
AU Thompson, KB
   Bateman, MG
   Carey, LD
AF Thompson, Kelsey B.
   Bateman, Monte G.
   Carey, Lawrence D.
TI A Comparison of Two Ground-Based Lightning Detection Networks against
   the Satellite-Based Lightning Imaging Sensor (LIS)
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID OPTICAL TRANSIENT DETECTOR; LOCATION NETWORK; PERFORMANCE ASSESSMENT;
   DETECTION EFFICIENCY; MAPPING ARRAY; WWLLN; ALGORITHM; ACCURACY; SYSTEM
AB Lightning stroke data from both the World Wide Lightning Location Network (WWLLN) and the Earth Networks Total Lightning Network (ENTLN) were compared to lightning group data from the Lightning Imaging Sensor (LIS) from 1 January 2010 through 30 June 2011. The region of study, from 39 degrees S to 39 degrees N latitude, chosen based on the orbit of LIS, and 164 E east to 17 W longitude, chosen to approximate the possible Geostationary Lightning Mapper (GLM) longitude, was considered in its entirety and then divided into geographical subregions. Over this 18-month time period, WWLLN had an 11.0% entire region, 13.2% North American, 6.2% South American, 16.4% Atlantic Ocean, and 18.9% Pacific Ocean coincidence percent (CP) value. The ENTLN CP values were 28.5%, 63.3%, 2.2%, 3.0%, and 2.5%, respectively. During the 18 months, WWLLN CP values remained rather consistent but low and often higher over ocean than land; ENTLN CP values showed large spatial and temporal variability. With both networks, North America had less variability during summer months than winter months and higher CP values during winter months than summer months. The highest ENTLN CP values were found in the southeastern United States, especially in a semicircle that extended from central Oklahoma, through Texas, along the northern Gulf of Mexico, across southern Florida, and along the U.S. East Coast. There was no significant change in CP values over time; the lowest monthly North American ENTLN CP value was found in June 2011 at 48.1%, the last month analyzed. These findings are consistent with most ENTLN sensors being located in the United States.
C1 [Thompson, Kelsey B.; Carey, Lawrence D.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA.
   [Bateman, Monte G.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
RP Thompson, KB (reprint author), Univ Alabama, Dept Atmospher Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM kelsey.thompson@nsstc.uah.edu
FU National Oceanic and Atmospheric Administration (NOAA) Geostationary
   Operational Environmental Satellite R series (GOES-R) Algorithm Working
   Group (AWG)
FX This work was funded by the National Oceanic and Atmospheric
   Administration (NOAA) Geostationary Operational Environmental Satellite
   R series (GOES-R) Algorithm Working Group (AWG). We thank NOAA AWG
   Manager Jaime Daniels and senior (chief) scientist for the GOES-R System
   Program, Steven Goodman, for their guidance throughout all phases of
   this work effort. The authors wish to thank the World Wide Lightning
   Location Network (http://wwIIn.net), a collaboration among over 50
   universities and institutions, for providing the lightning location data
   used in this paper. We thank Earth Networks for its collaboration and
   for providing ENTLN data.
NR 27
TC 8
Z9 8
U1 4
U2 15
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 2014
VL 31
IS 10
BP 2191
EP 2205
DI 10.1175/JTECH-D-13-00186.1
PG 15
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA AQ8JJ
UT WOS:000343071500013
ER

PT J
AU Timm, AU
   Roberti, DR
   Streck, NA
   de Goncalves, LGG
   Acevedo, OC
   Moraes, OLL
   Moreira, VS
   Degrazia, GA
   Ferlan, M
   Toll, DL
AF Timm, Andrea Ucker
   Roberti, Debora R.
   Streck, Nereu Augusto
   de Goncalves, Luis Gustavo G.
   Acevedo, Otavio Costa
   Moraes, Osvaldo L. L.
   Moreira, Virnei S.
   Degrazia, Gervasio Annes
   Ferlan, Mitja
   Toll, David L.
TI Energy Partitioning and Evapotranspiration over a Rice Paddy in Southern
   Brazil
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID LAND-SURFACE PROCESSES; EVAPORATION METHODS; FLUX MEASUREMENTS;
   IMBALANCE PROBLEM; PAN EVAPORATION; BALANCE; EXCHANGE; MODELS; CARBON;
   AGROECOSYSTEM
AB During approximately 80% of its growing season, lowland flooded irrigated rice ecosystems in southern Brazil are kept within a 5-10-cm water layer. These anaerobic conditions have an influence on the partitioning of the energy and water balance components. Furthermore, this cropping system differs substantially from any other upland nonirrigated or irrigated crop ecosystems. In this study, daily, seasonal, and annual dynamics of the energy and water balance components were analyzed over a paddy rice farm in a subtropical location in southern Brazil using eddy covariance measurements. In this region, rice is grown once a year in low wetlands while the ground is kept fallow during the remaining of the year. Results show that the energy budget residual corresponded to up to 20% of the net radiation during the rice-growing season and around 10% for the remainder of the year (fallow). The energy and water balance analysis also showed that because of the high water table in the region, soil was near saturation most of the time, and latent heat flux dominated over sensible heat flux by up to one order of magnitude in some cases. The estimate of evapotranspiration ET using the crop coefficient multiplied by the reference evapotranspiration KcETo and the Penman-Monteith equation ETPM, describing the canopy resistance through leaf area index (LAI) obtained by remote sensing, represent well the measured evapotranspiration, mainly in the fallow periods. Therefore, using a specific crop parameter like LAI and crop height can be an easy and interesting alternative to estimate ET in vegetated lowland areas.
C1 [Timm, Andrea Ucker] Fac Serra Gaucha, Caxias Do Sul, RS, Brazil.
   [Roberti, Debora R.; Moraes, Osvaldo L. L.; Degrazia, Gervasio Annes] Univ Fed Santa Maria, Dept Phys, BR-97105900 Santa Maria, RS, Brazil.
   [Streck, Nereu Augusto] Univ Fed Santa Maria, Dept Phys, Dept Fitotecnia, BR-97105900 Santa Maria, RS, Brazil.
   [de Goncalves, Luis Gustavo G.; Moraes, Osvaldo L. L.] Inst Nacl Pesquisas Espaciais, Ctr Previstio Tempo & Estudos Climat, Sao Paulo, Brazil.
   [Moreira, Virnei S.] Univ Fed Pampa, Itaqui, RS, Brazil.
   [Ferlan, Mitja] Slovenian Forestry Inst, Ljubljana, Slovenia.
   [Toll, David L.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
RP Roberti, DR (reprint author), Univ Fed Santa Maria, Dept Phys, Av Roraima 1000, BR-97105900 Santa Maria, RS, Brazil.
EM debora@ufsm.br
FU National Council for Scientific and Technological Development (CNPq,
   Brazil); Coordination for the Improvement of Higher Education Personnel
   (CAPES, Brazil); Foundation for Research of Rio Grande do Sul State
   (FAPERGS); NASA [NNH08ZDA001N-DECISIONS]
FX The authors acknowledge the National Council for Scientific and
   Technological Development (CNPq, Brazil), the Coordination for the
   Improvement of Higher Education Personnel (CAPES, Brazil), the
   Foundation for Research of Rio Grande do Sul State (FAPERGS), and NASA
   for the project "Integrating NASA Earth Sciences Research Results into
   Decision Support Systems for Agriculture and Water Management in South
   America" (Grant NNH08ZDA001N-DECISIONS) for their financial support.
NR 41
TC 3
Z9 3
U1 4
U2 31
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 2014
VL 15
IS 5
BP 1975
EP 1988
DI 10.1175/JHM-D-13-0156.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AQ7AG
UT WOS:000342964400015
ER

PT J
AU Woike, MR
   Abdul-Aziz, A
AF Woike, Mark R.
   Abdul-Aziz, Ali
TI SENSORS Noncontact Sensor Technology for Propulsion Health Monitoring
SO MATERIALS EVALUATION
LA English
DT Article
C1 [Woike, Mark R.; Abdul-Aziz, Ali] NASA, Opt & Photon Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Woike, MR (reprint author), NASA, Opt & Photon Branch, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA.
EM mark.r.woike@nasa.gov; ali.abdul-aziz-1@nasa.gov
NR 12
TC 0
Z9 0
U1 0
U2 1
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 OCT
PY 2014
VL 72
IS 10
BP 1196
EP 1203
PG 8
WC Materials Science, Characterization & Testing
SC Materials Science
GA AR1HI
UT WOS:000343335900002
ER

PT J
AU Dietrich, DL
   Nayagam, V
   Hicks, MC
   Ferkul, PV
   Dryer, FL
   Farouk, T
   Shaw, BD
   Suh, HK
   Choi, MY
   Liu, YC
   Avedisian, CT
   Williams, FA
AF Dietrich, Daniel L.
   Nayagam, Vedha
   Hicks, Michael C.
   Ferkul, Paul V.
   Dryer, Frederick L.
   Farouk, Tanvir
   Shaw, Benjamin D.
   Suh, Hyun Kyu
   Choi, Mun Y.
   Liu, Yu Cheng
   Avedisian, C. Thomas
   Williams, Forman A.
TI Droplet Combustion Experiments Aboard the International Space Station
SO MICROGRAVITY SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Combustion; Droplet combustion; Microgravity; International space
   station; Experiments; Fire safety
ID MICROGRAVITY CONDITIONS; ATMOSPHERIC-PRESSURE; N-HEPTANE; EXTINCTION;
   METHANOL; FLAMES
AB This paper summarizes the first results from isolated droplet combustion experiments performed on the International Space Station (ISS). The long durations of microgravity provided in the ISS enable the measurement of droplet and flame histories over an unprecedented range of conditions. The first experiments were with heptane and methanol as fuels, initial droplet droplet diameters between 1.5 and 5.0 m m, ambient oxygen mole fractions between 0.1 and 0.4, ambient pressures between 0.7 and 3.0 a t m and ambient environments containing oxygen and nitrogen diluted with both carbon dioxide and helium. The experiments show both radiative and diffusive extinction. For both fuels, the flames exhibited pre-extinction flame oscillations during radiative extinction with a frequency of approximately 1 H z. The results revealed that as the ambient oxygen mole fraction was reduced, the diffusive-extinction droplet diameter increased and the radiative-extinction droplet diameter decreased. In between these two limiting extinction conditions, quasi-steady combustion was observed. Another important measurement that is related to spacecraft fire safety is the limiting oxygen index (LOI), the oxygen concentration below which quasi-steady combustion cannot be supported. This is also the ambient oxygen mole fraction for which the radiative and diffusive extinction diameters become equal. For oxygen/nitrogen mixtures, the LOI is 0.12 and 0.15 for methanol and heptane, respectively. The LOI increases to approximately 0.14 (0.14 O (2)/0.56 N (2)/0.30 C O (2)) and 0.17 (0.17 O (2)/0.63 N (2)/0.20 C O (2)) for methanol and heptane, respectively, for ambient environments that simulated dispersing an inert-gas suppressant (carbon dioxide) into a nominally air (1.0 a t m) ambient environment. The LOI is approximately 0.14 and 0.15 for methanol and heptane, respectively, when helium is dispersed into air at 1 atm. The experiments also showed unique burning behavior for large heptane droplets. After the visible hot flame radiatively extinguished around a large heptane droplet, the droplet continued to burn with a cool flame. This phenomena was observed repeatably over a wide range of ambient conditions. These cool flames were invisible to the experiment imaging system but their behavior was inferred by the sustained quasi-steady burning after visible flame extinction. Verification of this new burning regime was established by both theoretical and numerical analysis of the experimental results. These innovative experiments have provided a wealth of new data for improving the understanding of droplet combustion and related aspects of fire safety, as well as offering important measurements that can be used to test sophisticated evolving computational models and theories of droplet combustion.
C1 [Dietrich, Daniel L.; Hicks, Michael C.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
   [Nayagam, Vedha] Case Western Reserve Univ, Cleveland, OH 44106 USA.
   [Ferkul, Paul V.] Univ Space Res Assoc, Cleveland, OH USA.
   [Dryer, Frederick L.] Princeton Univ, Princeton, NJ 08544 USA.
   [Farouk, Tanvir] Univ S Carolina, Columbia, SC 29208 USA.
   [Shaw, Benjamin D.] Univ Calif Davis, Davis, CA 95616 USA.
   [Suh, Hyun Kyu; Choi, Mun Y.] Kongju Natl Univ, Chunan, South Korea.
   [Liu, Yu Cheng; Avedisian, C. Thomas] Cornell Univ, Ithaca, NY USA.
   [Williams, Forman A.] Univ Calif San Diego, San Diego, CA 92103 USA.
RP Dietrich, DL (reprint author), NASA, John H Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
EM Daniel.L.Dietrich@nasa.gov; hksuh@kongju.ac.kr
NR 29
TC 13
Z9 13
U1 6
U2 27
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0938-0108
EI 1875-0494
J9 MICROGRAVITY SCI TEC
JI Microgravity Sci. Technol.
PD OCT
PY 2014
VL 26
IS 2
BP 65
EP 76
DI 10.1007/s12217-014-9372-2
PG 12
WC Engineering, Aerospace; Thermodynamics; Mechanics
SC Engineering; Thermodynamics; Mechanics
GA AQ8DT
UT WOS:000343054400001
ER

PT J
AU Hegglin, MI
   Plummer, DA
   Shepherd, TG
   Scinocca, JF
   Anderson, J
   Froidevaux, L
   Funke, B
   Hurst, D
   Rozanov, A
   Urban, J
   von Clarmann, T
   Walker, KA
   Wang, HJ
   Tegtmeier, S
   Weigel, K
AF Hegglin, M. I.
   Plummer, D. A.
   Shepherd, T. G.
   Scinocca, J. F.
   Anderson, J.
   Froidevaux, L.
   Funke, B.
   Hurst, D.
   Rozanov, A.
   Urban, J.
   von Clarmann, T.
   Walker, K. A.
   Wang, H. J.
   Tegtmeier, S.
   Weigel, K.
TI Vertical structure of stratospheric water vapour trends derived from
   merged satellite data
SO NATURE GEOSCIENCE
LA English
DT Article
ID BREWER-DOBSON CIRCULATION; TROPICAL TROPOPAUSE LAYER; TEMPERATURE
   TRENDS; UPPER TROPOSPHERE; TIME-SERIES; ERA-INTERIM; VARIABILITY;
   DEHYDRATION; VALIDATION; ATMOSPHERE
AB Stratospheric water vapour is a powerful greenhouse gas. The longest available record from balloon observations over Boulder, Colorado, USA shows increases in stratospheric water vapour concentrations that cannot be fully explained by observed changes in the main drivers, tropical tropopause temperatures and methane. Satellite observations could help resolve the issue, but constructing a reliable long-term data record from individual short satellite records is challenging. Here we present an approach to merge satellite data sets with the help of a chemistry-climate model nudged to observed meteorology. We use the models' water vapour as a transfer function between data sets that overcomes issues arising from instrument drift and short overlap periods. In the lower stratosphere, our water vapour record extends back to 1988 and water vapour concentrations largely follow tropical tropopause temperatures. Lower and mid-stratospheric long-term trends are negative, and the trends from Boulder are shown not to be globally representative. In the upper stratosphere, our record extends back to 1986 and shows positive long-term trends. The altitudinal differences in the trends are explained by methane oxidation together with a strengthened lower-stratospheric and a weakened upper-stratospheric circulation inferred by this analysis. Our results call into question previous estimates of surface radiative forcing based on presumed global long-term increases in water vapour concentrations in the lower stratosphere.
C1 [Hegglin, M. I.; Shepherd, T. G.] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England.
   [Plummer, D. A.; Scinocca, J. F.] Canadian Ctr Climate Modelling & Anal, Victoria, BC V8W 3V6, Canada.
   [Anderson, J.] Hampton Univ, Hampton, VA 23668 USA.
   [Froidevaux, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91020 USA.
   [Funke, B.] Inst Astrofis Andalucia, E-18080 Granada, Spain.
   [Hurst, D.] NOAA, Earth Syst Res Lab, Global Monitoring Div, Boulder, CO 80305 USA.
   [Rozanov, A.; Weigel, K.] Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany.
   [Urban, J.] Chalmers, Dept Earth & Space Sci, S-41296 Gothenburg, Sweden.
   [von Clarmann, T.] Karlsruhe Inst Technol, D-76021 Karlsruhe, Germany.
   [Walker, K. A.] Univ Toronto, Toronto, ON M5S 1A7, Canada.
   [Wang, H. J.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
   [Tegtmeier, S.] GEOMAR, D-24105 Kiel, Germany.
RP Hegglin, MI (reprint author), Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England.
EM m.i.hegglin@reading.ac.uk
RI Funke, Bernd/C-2162-2008; Hegglin, Michaela/D-7528-2017
OI Funke, Bernd/0000-0003-0462-4702; Hegglin, Michaela/0000-0003-2820-9044
FU Canadian Space Agency [CMAM30]
FX We acknowledge the Canadian Space Agency for funding the CMAM30 project,
   with additional institutional support from the Canadian Centre for
   Climate Modelling and Analysis, who provided the model code and
   supercomputing time. We thank all national and international space
   agencies for making available their limb satellite observations for use
   in the SPARC Data Initiative.
NR 47
TC 45
Z9 45
U1 0
U2 33
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 OCT
PY 2014
VL 7
IS 10
BP 768
EP 776
DI 10.1038/NGEO2236
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA AQ8VC
UT WOS:000343112600024
ER

PT J
AU Bussieres, F
   Clausen, C
   Tiranov, A
   Korzh, B
   Verma, VB
   Nam, SW
   Marsili, F
   Ferrier, A
   Goldner, P
   Herrmann, H
   Silberhorn, C
   Sohler, W
   Afzelius, M
   Gisin, N
AF Bussieres, Felix
   Clausen, Christoph
   Tiranov, Alexey
   Korzh, Boris
   Verma, Varun B.
   Nam, Sae Woo
   Marsili, Francesco
   Ferrier, Alban
   Goldner, Philippe
   Herrmann, Harald
   Silberhorn, Christine
   Sohler, Wolfgang
   Afzelius, Mikael
   Gisin, Nicolas
TI Quantum teleportation from a telecom-wavelength photon to a solid-state
   quantum memory
SO NATURE PHOTONICS
LA English
DT Article
ID ATOMIC-ENSEMBLE; QUBITS; REPEATERS; SYSTEM; MATTER; LIGHT
AB Quantum teleportation(1) is a cornerstone of quantum information science due to its essential role in important tasks such as the long-distance transmission of quantum information using quantum repeaters(2,3). This requires the efficient distribution of entanglement between remote nodes of a network(4). Here, we demonstrate quantum teleportation of the polarization state of a telecom-wavelength photon onto the state of a solid-state quantum memory. Entanglement is established between a rare-earth-ion-doped crystal storing a single photon that is polarization-entangled with a flying telecom-wavelength photon(5,6). The latter is jointly measured with another flying polarization qubit to be teleported, which heralds the teleportation. The fidelity of the qubit retrieved from the memory is shown to be greater than the maximum fidelity achievable without entanglement, even when the combined distances travelled by the two flying qubits is 25 km of standard optical fibre. Our results demonstrate the possibility of long-distance quantum networks with solid-state resources.
C1 [Bussieres, Felix; Clausen, Christoph; Tiranov, Alexey; Korzh, Boris; Gisin, Nicolas] Univ Geneva, Grp Appl Phys, CH-1211 Geneva 4, Switzerland.
   [Verma, Varun B.; Nam, Sae Woo] NIST, Boulder, CO 80305 USA.
   [Marsili, Francesco] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Ferrier, Alban; Goldner, Philippe] PSL Res Univ, Chim ParisTech, CNRS, Inst Rech Chim Paris, F-75005 Paris, France.
   [Ferrier, Alban] UPMC Univ Paris 06, Sorbonne Univ, F-75005 Paris, France.
   [Herrmann, Harald; Silberhorn, Christine; Sohler, Wolfgang] Univ Paderborn, Appl Phys Integrated Opt Grp, D-33095 Paderborn, Germany.
RP Bussieres, F (reprint author), Univ Geneva, Grp Appl Phys, CH-1211 Geneva 4, Switzerland.
EM felix.bussieres@unige.ch
RI Tiranov, Alexey/A-1453-2015; Herrmann, Hartmut/C-2486-2009; Silberhorn,
   Christine/J-4919-2013; Bussieres, Felix/E-5384-2011; Afzelius,
   Mikael/N-5825-2016
OI Herrmann, Hartmut/0000-0001-7044-2101; Silberhorn,
   Christine/0000-0002-2349-5443; Bussieres, Felix/0000-0003-0234-175X;
   Afzelius, Mikael/0000-0001-8367-6820
FU European project QuReP; Swiss National Centre of Competence in Research
   'Quantum Science and Technology' (NCCR QSIT)
FX The authors thank R. Thew, P. Sekatski and H. Zbinden for discussions.
   The authors acknowledge support by the European project QuReP and the
   Swiss National Centre of Competence in Research 'Quantum Science and
   Technology' (NCCR QSIT). 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 30
TC 58
Z9 60
U1 7
U2 56
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1749-4885
EI 1749-4893
J9 NAT PHOTONICS
JI Nat. Photonics
PD OCT
PY 2014
VL 8
IS 10
DI 10.1038/NPHOTON.2014.215
PG 4
WC Optics; Physics, Applied
SC Optics; Physics
GA AQ9DU
UT WOS:000343145200010
ER

PT J
AU Campbell, JF
AF Campbell, Joel F.
TI A low cost remote sensing system using PC and stereo equipment (vol 79,
   pg 1240, 2011)
SO AMERICAN JOURNAL OF PHYSICS
LA English
DT Correction
ID LASER SYSTEM
C1 NASA, Langley Res Ctr, Hampton, VA 23662 USA.
RP Campbell, JF (reprint author), NASA, Langley Res Ctr, Hampton, VA 23662 USA.
EM joel.f.campbell@nasa.gov
NR 9
TC 0
Z9 0
U1 0
U2 0
PU AMER ASSOC PHYSICS TEACHERS AMER INST PHYSICS
PI MELVILLE
PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA
SN 0002-9505
EI 1943-2909
J9 AM J PHYS
JI Am. J. Phys.
PD OCT
PY 2014
VL 82
IS 10
BP 1000
EP 1002
DI 10.1119/1.4883220
PG 3
WC Education, Scientific Disciplines; Physics, Multidisciplinary
SC Education & Educational Research; Physics
GA AQ5AI
UT WOS:000342813900013
ER

PT J
AU Volz, MP
   Mazuruk, K
AF Volz, M. P.
   Mazuruk, K.
TI Shape evolution of detached Bridgman crystals grown in microgravity
SO CRYSTAL RESEARCH AND TECHNOLOGY
LA English
DT Article
DE Bridgman growth; detached growth; dewetting; microgravity
ID DEWETTED BRIDGMAN; ANGLE; MELT
AB Detached (or dewetted) Bridgman crystal growth defines that process in which a gap exists between a growing crystal and the crucible wall. In microgravity, the parameters that influence the existence of a stable gap are the growth angle of the solidifying crystal, the contact angle between the melt and the crucible wall, and the pressure difference across the meniscus. During actual crystal growth, the initial crystal radius will not have the precise value required for stable detached growth. Beginning with a crystal diameter that differs from stable conditions, numerical calculations are used to analyze the transient crystal growth process. Depending on the initial conditions and growth parameters, the crystal shape will either evolve towards attachment at the crucible wall, towards a stable gap width, or inwards towards eventual collapse of the meniscus. Dynamic growth stability is observed only when the sum of the growth and contact angles exceeds 180 degrees.
C1 [Volz, M. P.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
   [Mazuruk, K.] Univ Alabama, Huntsville, AL 35899 USA.
RP Volz, MP (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM Martin.Volz@nasa.gov
FU U. S. National Aeronautics and Space Administration [NNM11AA01A]
FX This research was supported by the U. S. National Aeronautics and Space
   Administration under cooperative agreement NNM11AA01A.
NR 18
TC 1
Z9 1
U1 2
U2 6
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 0232-1300
EI 1521-4079
J9 CRYST RES TECHNOL
JI Cryst. Res. Technol.
PD OCT
PY 2014
VL 49
IS 10
BP 768
EP 776
DI 10.1002/crat.201400116
PG 9
WC Crystallography
SC Crystallography
GA AQ4MF
UT WOS:000342770600003
ER

PT J
AU Noell, AC
   Abbey, WJ
   Anderson, RC
   Ponce, A
AF Noell, Aaron C.
   Abbey, William J.
   Anderson, Robert C.
   Ponce, Adrian
TI Radiocarbon dating of glacial dust layers and soils at Kilimanjaro's
   Northern Ice Field
SO HOLOCENE
LA English
DT Article
DE cryoconite; glacier; Kilimanjaro; Northern Ice Field; radiocarbon;
   supraglacial
ID EQUATORIAL EAST-AFRICA; CLIMATE-CHANGE; ORGANIC-MATTER; MASS-BALANCE;
   RECORDS; CORE; PALEOCLIMATE; TERRESTRIAL; AEROSOLS; HOLOCENE
AB As the African climate history recorded in Kilimanjaro's Northern Ice Field (NIF) is rapidly lost, the age of the glacier remains disputed. Current age estimates from ice core data and glacial dynamics modeling disagree by an order of magnitude (11,700 vs similar to 1000 years old). We present radiocarbon dates of glacial dust and proximal soil samples collected from in and around the edge of the NIF that support the hypothesis that the peripheral portions of the NIF glacier are younger and more dynamic than the center. Samples of a dust-rich ice layer, 1.5m above the base at the edge of the similar to 40m high glacier ice cliff were found to be 1600-790 years old. These dates agree with the prediction of significant growth and shrinkage in glacial coverage over the last millennium. The variation in radiocarbon ages likely arises from heterogeneity in the summit volcanic soils, the main source of the dust recovered from the glacier, and cryoconite microbial activity. Sediment samples of a supraglacial pond had modern radiocarbon ages, further demonstrating the impact of cryoconite microbial communities on radiocarbon measurements of glacial samples. After accounting for the variability in the sample ages and the effects of microbial activity, we contend that the lower (i.e. younger) limit of the radiocarbon age range is the most reliable assessment of the age of the ice in which it was trapped.
C1 [Noell, Aaron C.; Abbey, William J.; Anderson, Robert C.; Ponce, Adrian] CALTECH, Pasadena, CA 91109 USA.
RP Ponce, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Adrian.Ponce@jpl.nasa.gov
FU NASA; Icy Worlds NASA Astrobiology Institute
FX Funding support was provided by the NASA Postdoctoral Program and Icy
   Worlds NASA Astrobiology Institute. 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 ((c) 2013 California Institute of Technology). Government
   sponsorship is acknowledged.
NR 50
TC 1
Z9 1
U1 0
U2 9
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0959-6836
EI 1477-0911
J9 HOLOCENE
JI Holocene
PD OCT
PY 2014
VL 24
IS 10
BP 1398
EP 1405
DI 10.1177/0959683614540945
PG 8
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA AQ4ZB
UT WOS:000342809500019
ER

PT J
AU Smith, GL
   Doelling, DR
AF Smith, G. Louis
   Doelling, David R.
TI Computation of Radiation Budget on an Oblate Earth
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Coordinate systems
ID ENERGY SYSTEM CERES; CLOUDS
AB The effects of the earth's oblateness on computation of its radiation budget from satellite measurements are evaluated. For the Clouds and the Earth's Radiant Energy System (CERES) data processing, geolocations of the measurements are computed in terms of the geodetic coordinate system. Using this system accounts for oblateness in the computed solar zenith angle and length of day. The geodetic and geocentric latitudes are equal at the equator and poles but differ by a maximum of 0.2 degrees at 45 degrees latitude. The area of each region and zone is affected by oblateness as compared to geocentric coordinates, decreasing from zero at the equator to 1.5% at the poles. The global area receiving solar radiation is calculated using the equatorial and polar axes. This area varies with solar declination by 0.0005. For radiation budget computations, the earth oblateness effects are shown to be small compared to error sources of measuring or modeling.
C1 [Smith, G. Louis] Sci Syst Applicat Inc, Hampton, VA USA.
   [Doelling, David R.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Smith, GL (reprint author), Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM george.l.smith@nasa.gov
FU Sciences Directorate of Langley Research Center; NASA Science Mission
   Directorate
FX The authors acknowledge support for this work by the Sciences
   Directorate of Langley Research Center and the NASA Science Mission
   Directorate.
NR 7
TC 0
Z9 0
U1 0
U2 4
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 OCT
PY 2014
VL 27
IS 19
BP 7203
EP 7206
DI 10.1175/JCLI-D-14-00058.1
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AQ5ID
UT WOS:000342840400002
ER

PT J
AU Huang, XL
   Chen, XH
   Potter, GL
   Oreopoulos, L
   Cole, JNS
   Lee, D
   Loeb, NG
AF Huang, Xianglei
   Chen, Xiuhong
   Potter, Gerald L.
   Oreopoulos, Lazaros
   Cole, Jason N. S.
   Lee, Dongmin
   Loeb, Norman G.
TI A Global Climatology of Outgoing Longwave Spectral Cloud Radiative
   Effect and Associated Effective Cloud Properties
SO JOURNAL OF CLIMATE
LA English
DT Article
DE Cloud radiative effects; Longwave radiation; Satellite observations;
   General circulation models; Model evaluation; performance
ID ANGULAR-DISTRIBUTION MODELS; ENERGY SYSTEM INSTRUMENT; TERRA SATELLITE;
   FLUX ESTIMATION; DATA PRODUCTS; TOP PRESSURE; ISCCP DATA; PART I;
   TEMPERATURE; CIRCULATION
AB Longwave (LW) spectral flux and cloud radiative effect (CRE) are important for understanding the earth's radiation budget and cloud-radiation interaction. Here, the authors extend their previous algorithms to collocated Atmospheric Infrared Sounder (AIRS) and Cloud and the Earth's Radiant Energy System (CERES) observations over the entire globe and show that the algorithms yield consistently good performances for measurements over both land and ocean. As a result, the authors are able to derive spectral flux and CRE at 10-cm(-1) intervals over the entire LW spectrum from all currently available collocated AIRS and CERES observations. Using this multiyear dataset, they delineate the climatology of spectral CRE, including the far IR, over the entire globe as well as in different climate zones. Furthermore, the authors define two quantities, IR-effective cloud-top height (CTHeff) and cloud amount (CA(eff)), based on the monthly-mean spectral (or band by band) CRE. Comparisons with cloud fields retrieved by the CERES-Moderate Resolution Imaging Spectroradiometer (MODIS) algorithm indicate that, under many circumstances, the CTHeff and CA(eff) can be related to the physical retrievals of CTH and CA and thus can enhance understandings of model deficiencies in LW radiation budgets and cloud fields. Using simulations from the GFDL global atmosphere model, version 2 (AM2); NASA's Goddard Earth Observing System, version 5 (GEOS-5); and Environment Canada's Canadian Centre for Climate Modelling and Analysis (CCCma) Fourth Generation Canadian Atmospheric General Circulation Model (CanAM4) as case studies, the authors further demonstrate the merits of the CTHeff and CA(eff) concepts in providing insights on global climate model evaluations that cannot be obtained solely from broadband LW flux and CRE comparisons.
C1 [Huang, Xianglei; Chen, Xiuhong; Potter, Gerald L.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
   [Oreopoulos, Lazaros; Lee, Dongmin] NASA, Div Earth Sci, Goddard Space Flight Ctr, Greenbelt, MD USA.
   [Cole, Jason N. S.] Environm Canada, Canadian Ctr Climate Modelling & Anal, Toronto, ON, Canada.
   [Lee, Dongmin] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA.
   [Loeb, Norman G.] NASA, Radiat & Climate Branch, Langley Res Ctr, Hampton, VA USA.
RP Huang, XL (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, 2455 Hayward St, Ann Arbor, MI 48109 USA.
EM xianglei@umich.edu
RI Huang, Xianglei/G-6127-2011; Oreopoulos, Lazaros/E-5868-2012; Chen,
   Xiuhong/P-4030-2014; 
OI Huang, Xianglei/0000-0002-7129-614X; Oreopoulos,
   Lazaros/0000-0001-6061-6905; Cole, Jason/0000-0003-0450-2748
FU NASA Terra/Aqua program [NNX11AH55G]; NASA's Modeling, Analysis, and
   Prediction Program
FX We wish to thank Dr. S. Tett and an anonymous reviewer for their
   thorough and thoughtful comments, which helped us greatly improve the
   clarity of the presentation. The Aqua CERES data were obtained from NASA
   Langley DAAC and AIRS level 1B data from NASA GSFC DAAC. The ECMWF
   ERA-Interim data are from
   http://data-portal.ecmwf.int/data/d/interim_daily/. The MODIS-CE data
   were from the Climserv Data Center of IPSL/CNRS. This research is
   supported by the NASA Terra/Aqua program under Grant NNX11AH55G awarded
   to the University of Michigan. L. Oreopoulos and D.M. Lee also
   acknowledge support by NASA's Modeling, Analysis, and Prediction
   Program.
NR 42
TC 5
Z9 5
U1 1
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD OCT
PY 2014
VL 27
IS 19
BP 7475
EP 7492
DI 10.1175/JCLI-D-13-00663.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AQ5ID
UT WOS:000342840400019
ER

PT J
AU Elliott, BM
   Sung, K
   Miller, CE
AF Elliott, Ben M.
   Sung, Keeyoon
   Miller, Charles E.
TI FT-IR spectra of O-17-enriched CO2 in the nu(3) region: High accuracy
   frequency calibration and spectroscopic constants for
   (OCO)-O-16-C-12-O-17, (OCO)-O-17-C-12-O-17, and (OCO)-O-17-C-12-O-18
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE O-17-enriched; CO2; FT-IR; Absolute calibration accuracy; Remote sensing
ID SENSITIVITY CAVITY RING; ENRICHED CARBON-DIOXIDE; CONSTRAINED
   MULTISPECTRUM ANALYSIS; 4.3 MU-M; 7000 CM(-1); INFRARED-SPECTROSCOPY;
   LINE POSITIONS; ABSORPTION-BANDS; SPEED DEPENDENCE; ISOTOPIC CO2
AB We report new Fourier transform infrared (FT-IR) spectroscopy measurements of the O-17-enriched isotopologues of CO2 in the v(3) region (2200-2450 cm(-1), 65-75 THz) with absolute calibration accuracies better than 3 x 10(-6) cm(-1) (similar to 100 kHz) for strong, isolated transitions. Spectra were obtained using the JPL Bruker IFS-125HR Fourier Transform Spectrometer (JPL-FTS). The JPL-FTS performance was achieved by vigorously maintaining the optical alignment, regularly monitoring its modulation efficiency while minimizing phase errors to deliver absolute frequency calibration and line position accuracies comparable to typical sub-millimeter/THz spectroscopy. Fits of the 00011 <- 00001 fundamental bands for (OCO)-O-16-C-12-O-17 (627), (OCO)-O-17-C-12-O-17 (727) and (OCO)-O-17-C-12-O-18 (728) were obtained with RMS residual values of 2.9 x 10(-6) cm(-1) for all three isotopologues. These results provide a complete and accurate set of transition frequencies required for remote sensing of planetary atmospheres, especially Venus and Mars, and represent a new level of Doppler measurement accuracies. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Elliott, Ben M.; Sung, Keeyoon; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Elliott, BM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ben.m.elliott@jpl.nasa.gov; keeyoon.sung@jpl.nasa.gov;
   charles.e.miller@jpl.nasa.gov
RI Sung, Keeyoon/I-6533-2015
FU NASA; National Aeronautics and Space Administration
FX BM Elliott was supported by an appointment to the NASA Postdoctoral
   Program at the Jet Propulsion Laboratory, California Institute of
   Technology, administered by Oak Ridge Associated Universities through a
   contract with NASA. The authors thank Timothy Crawford for his
   professional assistance in maintaining the JPL-FTS and all the
   peripheral apparatus. K Sung thanks Baron Vazindel from Bruker Optics,
   Inc. for his professional on-site service performance, especially on the
   optics alignment for the Bruker IFS-125HR at JPL since its installation
   in 2006. The research described in this paper was performed at the Jet
   Propulsion Laboratory, California Institute of Technology, under
   contract with the National Aeronautics and Space Administration.
   Copyright (C) 2014 California Institute of Technology. Government
   sponsorship acknowledged.
NR 50
TC 3
Z9 3
U1 1
U2 12
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 2014
VL 304
BP 1
EP 11
DI 10.1016/j.jms.2014.08.001
PG 11
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA AQ8IH
UT WOS:000343068700001
ER

PT J
AU Mantz, AW
   Sung, K
   Brown, LR
   Crawford, TJ
   Smith, MAH
   Devi, VM
   Benner, DC
AF Mantz, Arlan W.
   Sung, Keeyoon
   Brown, Linda R.
   Crawford, Timothy J.
   Smith, Mary Ann H.
   Devi, V. Malathy
   Benner, D. Chris
TI A cryogenic Herriott cell vacuum-coupled to a Bruker IFS-125HR
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Herriott cell; FT-IR; Bruker IFS-125HR; Cryogenic gas cell; Temperature
   dependence
ID INCLUDING TEMPERATURE DEPENDENCES; MU-M; LINE PARAMETERS; ABSORPTION
   CELL; STATE ENERGIES; 20 K; METHANE; BAND; SPECTRUM; REGION
AB A new cryogenic Herriott cell and associated transfer optics have been designed and fabricated at Connecticut College under contract with NASA Langley Research Center to operate for the first time with the broad-band Bruker IFS-125HR Fourier transform spectrometer at the Jet Propulsion Laboratory (JPL). This 0.375 m base-length optical cavity produces an absorption path length, at 293 K, of 20.941 (+/- 0.006) m. The Herriott cell, constructed from oxygen-free high conductivity copper, is placed inside its own vacuum enclosure, which is isolated from the transfer optics chamber by one CaF2 window and separately evacuated. The transfer optics chamber is in turn coupled to the sample compartment of the Bruker IFS-125HR holding another set of transfer optics. The entire spectrometer, including the transfer optics chamber can be evacuated to similar to 10 mTorr; the cell vacuum enclosure is cryogenically evacuated to pressures below 10(-6) Torr. A closed-cycle helium refrigerator cools the Herriott cell. Initially tested at Connecticut College for temperatures between 250 and 50 K, the system has successfully been in operation for over two years at JPL. The cell has been used for recording spectra between 75 and 250 K, achieving excellent temperature uniformity (+/- 0.15 K) and long term stability (< 0.05 K/day). Configured with a single indium-sealed CaF2 window, it has provided Doppler-limited infrared absorption spectra of a number of molecular species above 2000 cm(-1) to investigate detailed spectroscopic properties (e.g. molecular line parameters at temperatures and pressures relevant to planetary atmospheres). The design, performance and detailed characterization of the Herriott cell system are discussed. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Mantz, Arlan W.] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA.
   [Sung, Keeyoon; Brown, Linda R.; Crawford, Timothy J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Smith, Mary Ann H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
   [Devi, V. Malathy; Benner, D. Chris] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
RP Mantz, AW (reprint author), 325 Santander Court, Punta Gorda, FL 33950 USA.
EM awman@conncoll.edu
RI Sung, Keeyoon/I-6533-2015
NR 48
TC 8
Z9 8
U1 1
U2 12
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 2014
VL 304
BP 12
EP 24
DI 10.1016/j.jms.2014.07.006
PG 13
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA AQ8IH
UT WOS:000343068700002
ER

PT J
AU Babuscia, A
   Cheung, KM
AF Babuscia, Alessandra
   Cheung, Kar-Ming
TI Reaction to 'An approach to perform expert elicitation for engineering
   design risk analysis: methodology and experimental results' Response
SO JOURNAL OF THE ROYAL STATISTICAL SOCIETY SERIES A-STATISTICS IN SOCIETY
LA English
DT Letter
C1 [Babuscia, Alessandra; Cheung, Kar-Ming] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Babuscia, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Alessandra.Babuscia@jpl.nasa.gov
NR 7
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0964-1998
EI 1467-985X
J9 J R STAT SOC A STAT
JI J. R. Stat. Soc. Ser. A-Stat. Soc.
PD OCT
PY 2014
VL 177
IS 4
BP 984
EP 985
PG 2
WC Social Sciences, Mathematical Methods; Statistics & Probability
SC Mathematical Methods In Social Sciences; Mathematics
GA AQ4JS
UT WOS:000342762700009
ER

PT J
AU Suwa, Y
   Enoto, T
AF Suwa, Yudai
   Enoto, Teruaki
TI Anisotropic neutrino effect on magnetar spin: constraint on inner
   toroidal field
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE magnetic fields; neutrinos; radiative transfer; stars: magnetars;
   pulsars: general
ID X-RAY PULSARS; CORE-COLLAPSE SUPERNOVAE; STARS; EVOLUTION; REPEATERS;
   SPECTRUM; CHANDRA; DECAY
AB The ultrastrong magnetic field of magnetars modifies the neutrino cross-section due to the parity violation of the weak interaction and can induce asymmetric propagation of neutrinos. Such an anisotropic neutrino radiation transfers not only the linear momentum of a neutron star but also the angular momentum, if a strong toroidal field is embedded inside the stellar interior. As such, the hidden toroidal field implied by recent observations potentially affects the rotational spin evolution of new-born magnetars. We analytically solve the transport equation for neutrinos and evaluate the degree of anisotropy that causes the magnetar to spin-up or spin-down during the early neutrino cooling phase. Supposing that after the neutrino cooling phase the dominant process causing the magnetar spin-down is the canonical magnetic dipole radiation, we compare the solution with the observed present rotational periods of anomalous X-ray pulsars 1E 1841-045 and 1E 2259+586, whose poloidal (dipole) fields are similar to 10(15) and 10(14) G, respectively. Combining with the supernova remnant age associated with these magnetars, the present evaluation implies a rough constraint of global (average) toroidal field strength at B-phi less than or similar to 10(15) G.
C1 [Suwa, Yudai] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan.
   [Enoto, Teruaki] RIKEN Nishina Ctr, High Energy Astrophys Lab, Wako, Saitama 3510198, Japan.
   [Enoto, Teruaki] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Suwa, Y (reprint author), Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Oiwake Cho, Kyoto 6068502, Japan.
EM suwa@yukawa.kyoto-u.ac.jp
FU HPCI Strategic Program of Japanese MEXT; JSPS KAKENHI [24-3320]; 
   [25103511]
FX We thank the referee, U. Geppert, for providing constructive comments
   and help in improving the contents of this paper. YS would like to thank
   P. Cerda-Duran and N. Yasutake for informative discussions, K.
   Hotokezaka, T. Muranushi, and M. Suwa for comments, and J. White for
   proofreading. We also thank the Yukawa Institute for Theoretical Physics
   at Kyoto University, where part of this work was done during the
   workshop YITP-T-13-04 entitled 'Long-term Workshop on Supernovae and
   Gamma-Ray Bursts 2013'. YS is supported in part by Grant-in-Aid for
   Scientific Research on Innovative Areas (No. 25103511) and by HPCI
   Strategic Program of Japanese MEXT. TE is supported by JSPS KAKENHI,
   Grant-in-Aid for JSPS Fellows, 24-3320.
NR 31
TC 0
Z9 0
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 1
PY 2014
VL 443
IS 4
BP 3586
EP 3593
DI 10.1093/mnras/stu1442
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ6KX
UT WOS:000342922100057
ER

PT J
AU Symeonidis, M
   Georgakakis, A
   Page, MJ
   Bock, J
   Bonzini, M
   Buat, V
   Farrah, D
   Franceschini, A
   Thar, E
   Lutz, D
   Magnelli, B
   Magdis, G
   Oliver, SJ
   Pannella, M
   Paolillo, M
   Rosario, D
   Roseboom, IG
   Vaccari, M
   Villforth, C
AF Symeonidis, M.
   Georgakakis, A.
   Page, M. J.
   Bock, J.
   Bonzini, M.
   Buat, V.
   Farrah, D.
   Franceschini, A.
   Thar, E.
   Lutz, D.
   Magnelli, B.
   Magdis, G.
   Oliver, S. J.
   Pannella, M.
   Paolillo, M.
   Rosario, D.
   Roseboom, I. G.
   Vaccari, M.
   Villforth, C.
TI Linking the X-ray and infrared properties of star-forming galaxies at z
   < 1.5
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: general; galaxies: high-redshift;
   galaxies: starburst; submillimetre: general; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; DEEP-FIELD-SOUTH; MASS-METALLICITY RELATION;
   FORMATION RATE INDICATOR; 2-10 KEV LUMINOSITY; SIMILAR-TO 1;
   GOODS-SOUTH; VLT/FORS2 SPECTROSCOPY; EXTRAGALACTIC SURVEY; NUMBER COUNTS
AB We present the most complete study to date of the X-ray emission from star formation in high-redshift (median z = 0.7; z < 1.5), IR-luminous (L-IR = 10(10)-10(13) L circle dot) galaxies detected by Herschel's PACS and SPIRE instruments. For our purpose, we take advantage of the deepest X-ray data to date, the Chandra Deep Fields (North and South). Sources which host AGN are removed from our analysis by means of multiple AGN indicators. We find an AGN fraction of 18 +/- 2 per cent amongst our sample and note that AGN entirely dominate at values of log [L-X/L-IR] > -3 in both hard and soft X-ray bands. From the sources which are star formation dominated, only a small fraction are individually X-ray detected and for the bulk of the sample we calculate average X-ray luminosities through stacking. We find an average soft X-ray to infrared ratio of log < L-SX/L-IR > = -4.3 and an average hard X-ray to infrared ratio of log < L-HX/L-IR > =-3.8. We report that the X-ray/IR correlation is approximately linear through the entire range of L-IR and z probed and, although broadly consistent with the local (z < 0.1) one, it does display some discrepancies. We suggest that these discrepancies are unlikely to be physical, i.e. due to an intrinsic change in the X-ray properties of star-forming galaxies with cosmic time, as there is no significant evidence for evolution of the L-X/L-IR ratio with redshift. Instead, they are possibly due to selection effects and remaining AGN contamination. We also examine whether dust obscuration in the galaxy plays a role in attenuating X-rays from star formation, by investigating changes in the L-X/L-IR ratio as a function of the average dust temperature. We conclude that X-rays do not suffer any measurable attenuation in the host galaxy.
C1 [Symeonidis, M.; Oliver, S. J.] Univ Sussex, Dept Phys & Astron, Astron Ctr, Brighton BN1 9QH, E Sussex, England.
   [Symeonidis, M.; Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
   [Georgakakis, A.; Lutz, D.; Rosario, D.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany.
   [Bock, J.] CALTECH, Pasadena, CA 91125 USA.
   [Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Bonzini, M.] European So Observ, D-85748 Garching, Germany.
   [Buat, V.; Farrah, D.] Univ Aix Marseille, CNRS, Lab Astrophys Marseille, OAMP, F-13388 Marseille 13, France.
   [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
   [Franceschini, A.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
   [Thar, E.] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile.
   [Magnelli, B.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
   [Magdis, G.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
   [Pannella, M.] Univ Paris Diderot, Lab AIM, CEA DSM CNRS, Irfu Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
   [Pannella, M.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
   [Paolillo, M.] Univ Naples Federico II, Dipartimento Fis, CU Monte St Angelo, I-80126 Naples, Italy.
   [Paolillo, M.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy.
   [Roseboom, I. G.] Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
   [Vaccari, M.] Univ Western Cape, Astrophys Grp, Dept Phys, ZA-7535 Cape Town, South Africa.
   [Villforth, C.] Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
   [Villforth, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
RP Symeonidis, M (reprint author), Univ Sussex, Dept Phys & Astron, Astron Ctr, Brighton BN1 9QH, E Sussex, England.
EM m.symeonidis@ucl.ca.uk
RI Georgakakis, Antonis/K-4457-2013; Magdis, Georgios/C-7295-2014;
   Paolillo, Maurizio/J-1733-2012; Vaccari, Mattia/R-3431-2016; 
OI Magdis, Georgios/0000-0002-4872-2294; Paolillo,
   Maurizio/0000-0003-4210-7693; Vaccari, Mattia/0000-0002-6748-0577;
   Georgakakis, Antonis/0000-0002-3514-2442
FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France);
   ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA
   (USA); BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR
   (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain)
FX This paper uses data from Herschel's photometers SPIRE and PACS. 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). PACS has been developed by a consortium
   of institutes led by MPE (Germany) and including UVIE (Austria); KU
   Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany);
   INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This
   development has been supported by the funding agencies BMVIT (Austria),
   ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy)
   and CICYT/MCYT (Spain). The scientific results reported in this paper
   are based to a significant degree on observations made by the Chandra
   X-ray Observatory.
NR 101
TC 9
Z9 9
U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT 1
PY 2014
VL 443
IS 4
BP 3728
EP 3740
DI 10.1093/mnras/stu1441
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ6KX
UT WOS:000342922100068
ER

PT J
AU Miller, SAE
AF Miller, Steven A. E.
TI Toward a Comprehensive Model of Jet Noise Using an Acoustic Analogy
SO AIAA JOURNAL
LA English
DT Article
ID SHOCK-ASSOCIATED NOISE; SUPERSONIC JETS; MIXING NOISE; SOUND;
   PREDICTION; TURBULENCE; PROPAGATION; SCHEMES; FLOWS
AB An acoustic analogy is developed to predict the noise from jet flows. It contains two source models that independently predict the noise from turbulence and shock wave shear layer interactions. The acoustic analogy is based on the Euler equations and separates the sources from propagation. Propagation effects are taken into account by approximating the vector Green's function of the linearized Euler equations with the use of a locally parallel mean flow assumption. A statistical model of the two-point cross correlation of the velocity fluctuations is used to describe the turbulence. The acoustic analogy attempts to take into account the correct scaling of the sources for a wide range of nozzle pressures and temperature ratios. It does not make assumptions regarding fine-or large-scale turbulent noise sources, self-or shear noise, or convective amplification. The acoustic analogy is partially informed by three-dimensional steady Reynolds-averaged Navier-Stokes solutions that include the nozzle geometry. The predictions are compared with experiments of jets operating subsonically through supersonically and at unheated and heated temperatures. Predictions generally capture the scaling of both mixing noise and broadband shock-associated noise for the conditions examined, but some discrepancies remain, which are due to the accuracy of the steady Reynolds-averaged Navier-Stokes turbulence model closure, the equivalent sources, and the use of a simplified vector Green's function solver of the linearized Euler equations using a locally parallel mean flow.
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Miller, SAE (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
NR 52
TC 3
Z9 3
U1 1
U2 2
PU AMER INST AERONAUTICS  ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD OCT
PY 2014
VL 52
IS 10
BP 2143
EP 2164
DI 10.2514/1.J052809
PG 22
WC Engineering, Aerospace
SC Engineering
GA AQ4IR
UT WOS:000342759200004
ER

PT J
AU Doty, MJ
AF Doty, Michael J.
TI Investigation of Twin Jet Aeroacoustic Properties near a Hybrid
   Wing-Body Shield
SO AIAA JOURNAL
LA English
DT Article
AB In preparation for wind-tunnel acoustic experiments of a hybrid wing-body vehicle with two jet engine simulator units, a series of twin jet aeroacoustic investigations was conducted leading to increased understanding and risk mitigation. An existing twin jet nozzle system and a fabricated hybrid wing-body aft deck fuselage are combined for a 1.9% model scale study of jet nozzle spacing and jet cant angle effects, elevon deflection into the jet plume, and acoustic shielding by the fuselage body. Linear and phased array microphone measurements are made, and data processing includes the use of the deconvolution approach for the mapping of acoustic sources. Closely spaced twin jets with a 5 deg inward cant angle exhibit reduced noise levels compared with their parallel flow counterparts at similar and larger nozzle spacings. A 40 deg elevon deflection into the twin jet plume, which is required for hybrid wing-body ground rotation, can significantly increase upstream noise levels (more than 5 dB overall sound pressure level) with only minimal increases in the downstream direction. Lastly, deconvolution approach for the mapping of acoustic sources processing can resolve the noise source distribution of multiple shielded jet sources within the limits of the incoherent source assumption.
C1 NASA, Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23681 USA.
RP Doty, MJ (reprint author), NASA, Langley Res Ctr, Aeroacoust Branch, Mail Stop 461, Hampton, VA 23681 USA.
FU Environmentally Responsible Aviation Project within NASA's Integrated
   Systems Research Program
FX Funding from the Environmentally Responsible Aviation Project within
   NASA's Integrated Systems Research Program is gratefully acknowledged.
   The author sincerely thanks the entire Jet Noise Laboratory team for
   their efforts during these experiments. In addition, Gerald Plassman was
   extremely helpful in supporting inquiries regarding the deconvolution
   approach for the mapping of acoustic sources (DAMAS) processing.
   Discussions with Thomas Brooks and William Humphreys about DAMAS theory
   have also been very much appreciated.
NR 12
TC 1
Z9 1
U1 0
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 OCT
PY 2014
VL 52
IS 10
BP 2270
EP 2282
DI 10.2514/1.J052783
PG 13
WC Engineering, Aerospace
SC Engineering
GA AQ4IR
UT WOS:000342759200014
ER

PT J
AU Takahashi, F
   Abbott, A
   Murray, TM
   T'ien, JS
   Olson, SL
AF Takahashi, Fumiaki
   Abbott, Amber
   Murray, Timothy M.
   T'ien, James S.
   Olson, Sandra L.
TI Thermal response characteristics of fire blanket materials
SO FIRE AND MATERIALS
LA English
DT Article
DE forest fire; heat-blocking efficiency; ignition prevention; building
   structure protection; wildland-urban interface; aluminized fiberglass;
   amorphous silica; aramid fabric
ID PERFORMANCE
AB The thermal response characteristics of over 50 relatively thin (0.15-3.7mm) fire blanket materials from four different fiber groups (aramid, fiberglass, amorphous silica, and pre-oxidized carbon) and their composites have been investigated. A plain or coated fabric sample was subjected to a predominantly convective or radiant heat flux (up to 84kW/m(2)) using a Meker burner and a cone heater, respectively. In addition to conventional thermal protective performance ratings for protective clothing, two transient thermal response times (for the fabric back-side temperature to reach 300 degrees C and for the through-the-fabric heat flux to reach 13kW/m(2)) and a steady-state heat-blocking efficiency (HBE) were introduced for both convective and radiant heat sources. For most woven fabrics, the HBE values were approximately 70 +/- 10% for both convection and radiation and only mildly increased with the fabric thickness or the incident heat flux. Nonwoven (felt) fabrics with low thermal conductivity exhibited significantly better insulation (up to 87%) against convective heat. Highly reflective aluminized materials exhibited exceptionally high HBE values (up to 98%) for radiation, whereas carbon and charred aramid fabrics showed lower HBEs (down to 50%) because of efficient radiation absorption. A relatively thin fire blanket operating at high temperatures can efficiently block heat from a convective source by radiative emission (enhanced by its T-4-dependence and high surface emissivity) coupled with thermal insulation and from a radiant heat source by surface reflection while the aluminum surface layer remains. Copyright (c) 2013 John Wiley & Sons, Ltd.
C1 [Takahashi, Fumiaki; Abbott, Amber; Murray, Timothy M.; T'ien, James S.] Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA.
   [Olson, Sandra L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Takahashi, F (reprint author), Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA.
EM fxt13@case.edu
FU US Department of Homeland Security, Federal Emergency Management Agency
   [EMW-2007-FP-02677]
FX This work was supported by the US Department of Homeland Security,
   Federal Emergency Management Agency, Assistance to Firefighters Grant
   Program, Fire Prevention and Safety Grant (no. EMW-2007-FP-02677). The
   following students are acknowledged for their assistance in conducting
   the experiment: Mallory Miller, Jason Williams, Jacob Teets, Brian
   Guzek, Margaret Rybach (CWRU), and Wyatt Ratliff (Stanford University).
   Fire shelter materials were provided by Anthony Petrilli (USDA Forest
   Service). Some fabric samples and thermal conductivity data were
   provided by Auburn Manufacturing, Inc. An initial version of this paper
   was presented as 'Characteristics of fire blanket materials for
   structure protection in wildland-urban interface fires', VI
   International Conference on Forest Fire Research (D. X. Viegas, Ed.),
   Coimbra, Portugal, November 2010.
NR 61
TC 2
Z9 2
U1 2
U2 27
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0308-0501
EI 1099-1018
J9 FIRE MATER
JI Fire Mater.
PD OCT
PY 2014
VL 38
IS 6
BP 609
EP 638
DI 10.1002/fam.2202
PG 30
WC Materials Science, Multidisciplinary
SC Materials Science
GA AQ4FV
UT WOS:000342749600001
ER

PT J
AU Lang, SE
   Tao, WK
   Chern, JD
   Wu, D
   Li, XW
AF Lang, Stephen E.
   Tao, Wei-Kuo
   Chern, Jiun-Dar
   Wu, Di
   Li, Xiaowen
TI Benefits of a Fourth Ice Class in the Simulated Radar Reflectivities of
   Convective Systems Using a Bulk Microphysics Scheme
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID CLOUD-RESOLVING MODEL; ADVECTION TRANSPORT ALGORITHM; HIGH-RESOLUTION
   SIMULATION; SMALL IMPLICIT DIFFUSION; PART I; ENSEMBLE MODEL; STRATIFORM
   PRECIPITATION; SATELLITE-OBSERVATIONS; EXPLICIT MICROPHYSICS;
   ENVIRONMENT INTERFACE
AB Current cloud microphysical schemes used in cloud and mesoscale models range from simple one-moment to multimoment, multiclass to explicit bin schemes. This study details the benefits of adding a fourth ice class (frozen drops/hail) to an already improved single-moment three-class ice (cloud ice, snow, graupel) bulk microphysics scheme developed for the Goddard Cumulus Ensemble model. Besides the addition and modification of several hail processes from a bulk three-class hail scheme, further modifications were made to the three-ice processes, including allowing greater ice supersaturation and mitigating spurious evaporation/sublimation in the saturation adjustment scheme, allowing graupel/hail to transition to snow via vapor growth and hail to transition to graupel via riming, wet graupel to become hail, and the inclusion of a rain evaporation correction and vapor diffusivity factor. The improved three-ice snow/graupel size-mapping schemes were adjusted to be more stable at higher mixing ratios and to increase the aggregation effect for snow. A snow density mapping was also added.
   The new scheme was applied to an intense continental squall line and a moderate, loosely organized continental case using three different hail intercepts. Peak simulated reflectivities agree well with radar for both the intense and moderate cases and were superior to earlier three-ice versions when using a moderate and large intercept for hail, respectively. Simulated reflectivity distributions versus height were also improved versus radar in both cases compared to earlier three-ice versions. The bin-based rain evaporation correction affected the squall line more but overall the agreement among the reflectivity distributions was unchanged. The new scheme also improved the simulated surface rain-rate histograms.
C1 [Lang, Stephen E.; Tao, Wei-Kuo; Chern, Jiun-Dar; Wu, Di; Li, Xiaowen] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA.
   [Lang, Stephen E.; Wu, Di] Sci Syst & Applicat Inc, Lanham, MD USA.
   [Chern, Jiun-Dar] Univ Maryland, Earth Syst Sci & Interdisciplinary Ctr, College Pk, MD 20742 USA.
   [Li, Xiaowen] Morgan State Univ, Baltimore, MD 21239 USA.
RP Lang, SE (reprint author), NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Code 612, Greenbelt, MD 20771 USA.
EM stephen.e.lang@nasa.gov
RI Measurement, Global/C-4698-2015
FU NASA Precipitation Measurement Missions (PMMs); NASA Modeling, Analysis,
   and Prediction (MAP) Program; Office of Science (BER), DOE-Atmospheric
   System Research Interagency Agreement [DE-AI02-04ER63755]
FX This research was supported by the NASA Precipitation Measurement
   Missions (PMMs); the NASA Modeling, Analysis, and Prediction (MAP)
   Program; and the Office of Science (BER), DOE-Atmospheric System
   Research Interagency Agreement DE-AI02-04ER63755. The authors are
   grateful to Drs. Ramesh Kakar and David B. Considine at NASA
   headquarters (HQ) for their support of this research, Dr. Shaocheng Xie
   at Lawrence Livermore National Laboratory for providing the MC3E forcing
   data, Dr. Robert Cifelli for providing the LBA radar data, Dr. Karen
   Mohr for discussions on precipitation-surface flux interactions, and
   Drs. Toshihisa Matsui and Jainn J. Shi for implementing and testing the
   4ICE scheme in the Goddard satellite simulator and WRF, respectively. We
   would also like to thank Dr. Jason Milbrandt and two other anonymous
   reviewers for greatly helping us to improve the quality of the
   manuscript. Acknowledgment is also made to the NASA Goddard Space Flight
   Center and NASA Ames Research Center computing facilities, as well as to
   Dr. Tsengdar Lee at NASA HQ, for the computational resources used in
   this research. MC3E is a NASA-DOE joint field campaign.
NR 127
TC 13
Z9 13
U1 0
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD OCT
PY 2014
VL 71
IS 10
BP 3583
EP 3612
DI 10.1175/JAS-D-13-0330.1
PG 30
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AP9IR
UT WOS:000342394000002
ER

PT J
AU Johnston, CO
AF Johnston, Christopher O.
TI Influence of Radiative Absorption on Non-Boltzmann Modeling for Mars
   Entry
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
C1 NASA Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
RP Johnston, CO (reprint author), NASA Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA.
NR 15
TC 1
Z9 1
U1 0
U2 0
PU AMER INST AERONAUTICS  ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0887-8722
EI 1533-6808
J9 J THERMOPHYS HEAT TR
JI J. Thermophys. Heat Transf.
PD OCT
PY 2014
VL 28
IS 4
BP 795
EP 798
DI 10.2514/1.T4044
PG 4
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA AQ2LU
UT WOS:000342618400020
ER

PT J
AU Bosley, KL
   Miller, TW
   Brodeur, RD
   Bosley, KM
   Van Gaest, A
   Elz, A
AF Bosley, Keith L.
   Miller, Todd W.
   Brodeur, Richard D.
   Bosley, Katelyn M.
   Van Gaest, Ahna
   Elz, Anna
TI Feeding ecology of juvenile rockfishes off Oregon and Washington based
   on stomach content and stable isotope analyses
SO MARINE BIOLOGY
LA English
DT Article
ID NORTHERN CALIFORNIA CURRENT; FAMILY SCORPAENIDAE; CARBON ISOTOPES; GENUS
   SEBASTES; TROPHIC INTERACTIONS; BRITISH-COLUMBIA; DIET; VARIABILITY;
   LARVAE; ECOSYSTEM
AB The feeding habits of pelagic, juvenile rockfishes (Sebastes spp.) collected off Oregon in 2002, and Oregon and Washington in 2006, were examined using stomach content and stable isotope analyses. Sampling occurred along a series of transects across the shelf between Crescent City, California (Lat. 41A degrees 54.0'), and Newport, Oregon (Lat. 44A degrees 39.0'), in 2002, and off Willapa Bay, Washington (Lat. 46A degrees 40.0'), and the Columbia River, Oregon (Lat. 46A degrees 10.0'), in 2006. Species composition varied both years with distance from shore, but the predominant species were darkblotched (Sebastes crameri), canary (S. pinniger), yellowtail (2006 only; S. flavidus), and widow (S. entomelas) rockfishes. Stomach content analysis revealed that darkblotched rockfish had highly variable diets, and canary, yellowtail, and widow rockfishes exhibited a high degree of overlap in 2006. Multivariate analysis showed significant differences in diet based on distance from shore where caught, fish size, and species. Stable isotope analysis indicated that all species were feeding at about the same trophic level within each year, with a 1.5 aEuro degrees difference in delta N-15 between years and regions. The difference in delta N-15 values may indicate a greater contribution of mesotrophic zooplankton such as euphausiids, hyperiid amphipods, and chaetognaths to fish diets in 2006. Depleted C-13 values were indicative of diets based on primary production from a more offshore origin, suggesting that these rockfish had previously inhabited offshore waters. These results add to our understanding of some of the important environmental factors that affect young-of-the-year rockfishes during their pelagic phase.
C1 [Bosley, Keith L.] NOAA, Fishery Resource Anal & Monitoring Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
   [Brodeur, Richard D.] NOAA, Fish Ecol Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
   [Bosley, Katelyn M.] Oregon State Univ, Dept Fisheries & Wildlife, Hatfield Marine Sci Ctr, Newport, OR 97365 USA.
   [Van Gaest, Ahna] NOAA, Environm & Fisheries Sci Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
   [Elz, Anna] NOAA, Conservat Biol Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98112 USA.
RP Bosley, KL (reprint author), NOAA, Fishery Resource Anal & Monitoring Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2032 SE OSU Dr, Newport, OR 97365 USA.
EM keith.bosley@noaa.gov
FU NOAA Northwest Fisheries Science Center Internal Grants Program; U.S.
   Global Ocean Ecosystem Dynamics Northeast Pacific Program; Bonneville
   Power Administration
FX This study was funded through the NOAA Northwest Fisheries Science
   Center Internal Grants Program, U.S. Global Ocean Ecosystem Dynamics
   Northeast Pacific Program, and the Bonneville Power Administration.
   Comments from Chris Harvey, Aimee Keller, Chris Harrod, and two
   anonymous reviewers improved the manuscript considerably, as did edits
   from Karen Bosley. We also wish to thank Chris Harvey and Phil Levin for
   invaluable assistance obtaining funding, and R. Emmett, J. Fisher, T.
   Sandell, S. Pool, and P. Bentley for help in sampling. Special thanks to
   M. Kubo, W. Reichert, and K. Turk for help with the stable isotope
   analysis.
NR 64
TC 3
Z9 3
U1 2
U2 39
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 2014
VL 161
IS 10
BP 2381
EP 2393
DI 10.1007/s00227-014-2513-8
PG 13
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA AP9QT
UT WOS:000342415200016
ER

PT J
AU Beavis, NK
   Lang, TJ
   Rutledge, SA
   Lyons, WA
   Cummer, SA
AF Beavis, Nick K.
   Lang, Timothy J.
   Rutledge, Steven A.
   Lyons, Walter A.
   Cummer, Steven A.
TI Regional, Seasonal, and Diurnal Variations of Cloud-to-Ground Lightning
   with Large Impulse Charge Moment Changes
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID MESOSCALE CONVECTIVE COMPLEXES; NORTH-AMERICAN-MONSOON; CONTIGUOUS
   UNITED-STATES; GULF-STREAM; SPRITES; SYSTEM; PRECIPITATION; ELF;
   TROPOSPHERE; RAINFALL
AB The use of both total charge moment change (CMC) and impulse charge moment change (iCMC) magnitudes to assess the potential of a cloud-to-ground (CG) lightning stroke to induce a mesospheric sprite has been well described in the literature, particularly on a case study basis. In this climatological study, large iCMC discharges for thresholds of >100 and >300 C km in both positive and negative polarities are analyzed on a seasonal basis. Also presented are local solar time diurnal distributions in eight different regions covering the lower 48 states as well as the adjacent Atlantic Ocean, including the Gulf Stream.
   The seasonal maps show the predisposition of large positive iCMCs to dominate across the northern Great Plains, with large negative iCMCs favored in the southeastern United States year-round. During summer, the highest frequency of large positive iCMCs across the upper Midwest aligns closely with the preferred tracks of nocturnal mesoscale convective systems (MCSs). As iCMC values increase above 300 C km, the maximum shifts eastward of the 100 C km maximum in the central plains.
   Diurnal distributions in the eight regions support these conclusions, with a nocturnal peak in large iCMC discharges in the northern Great Plains and Great Lakes, an early to midafternoon peak in the Intermountain West and the southeastern United States, and a morning peak in large iCMC discharge activity over the Atlantic Ocean. Large negative iCMCs peak earlier in time than large positive iCMCs, which may be attributed to the growth of large stratiform charge reservoirs following initial convective development.
C1 [Beavis, Nick K.; Rutledge, Steven A.] Colorado State Univ, Ft Collins, CO 80523 USA.
   [Lang, Timothy J.] NASA, Marshall Spaceflight Ctr, Huntsville, AL USA.
   [Lyons, Walter A.] FMA Res Inc, Ft Collins, CO USA.
   [Cummer, Steven A.] Duke Univ, Durham, NC USA.
RP Rutledge, SA (reprint author), Colorado State Univ, 123 Lake St, Ft Collins, CO 80523 USA.
EM rutledge@atmos.colostate.edu
RI Cummer, Steven/A-6118-2008; 
OI Cummer, Steven/0000-0002-0002-0613; Lang, Timothy/0000-0003-1576-572X
FU Missile Defense Agency SBIR program; National Science Foundation
   [AGS-1010657]; DARPA under the Nimbus program
FX The authors gratefully acknowledge the support of Vaisala, Inc., in
   providing the National Lightning Detection Network Data on which the
   CMCN is built, as well as the support of the Missile Defense Agency SBIR
   program. The National Science Foundation provided support for this work
   under Grant AGS-1010657, and DARPA provided additional funding support
   under the Nimbus program. The authors also would like to extend thanks
   to the Radar Meteorology Group at Colorado State University for valuable
   scientific input, and especially Paul Hein for invaluable computing
   support. Thanks also to Prof. Russ Schumacher and four anonymous
   reviewers for insightful scientific input and suggestions. The views,
   opinions, and findings in this report are those of the authors, and
   should not be construed as an official NASA or U.S. government position,
   policy, or decision.
NR 52
TC 4
Z9 4
U1 0
U2 2
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 2014
VL 142
IS 10
BP 3666
EP 3682
DI 10.1175/MWR-D-14-00034.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AQ0OK
UT WOS:000342482400009
ER

PT J
AU Rodriguez, LF
   Reipurth, B
   Chiang, HF
AF Rodriguez, Luis F.
   Reipurth, Bo
   Chiang, Hsin-Fang
TI RADIO CONTINUUM SOURCES ASSOCIATED WITH THE HH 92 AND HH 34 JETS
SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA
LA English
DT Article
DE ISM: jets and outflows; radio continuum: stars; stars: formation; stars:
   mass-loss
ID HERBIG-HARO OBJECTS; YOUNG STELLAR OBJECTS; PROPER MOTIONS;
   ENERGY-SOURCES; ORION; STARS; HH-34; DUST; VARIABILITY; MILLIMETER
AB We present high angular resolution, high sensitivity 8.46 GHz (3.6 cm) radio continuum observations made toward the core of the HH 92 outflow with the Very Large Array in 2002-2003 and with the Expanded Very Large Array in 2011. We detect a group of three compact sources distributed in a region 2 '' in extension and discuss their nature. We conclude that one of the objects (VLA 1) is the exciting source of the giant outflow associated with HH 92. In the case of HH 34 we present new 43.3 GHz (7 mm) observations that reveal the presence of a structure associated with the exciting source and elongated perpendicularly to the highly collimated optical jet in the region. We propose that this 7 mm source is a circumstellar disk with radius of approximate to 180 AU and mass of approximate to 0.21 M-circle dot.
C1 [Rodriguez, Luis F.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Mexico City 04510, DF, Mexico.
   [Rodriguez, Luis F.] King Abdulaziz Univ, Fac Sci, Dept Astron, Jeddah, Saudi Arabia.
   [Reipurth, Bo; Chiang, Hsin-Fang] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA.
   [Reipurth, Bo; Chiang, Hsin-Fang] Univ Hawaii Manoa, Astrobiol Inst, NASA, Hilo, HI USA.
RP Rodriguez, LF (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Campus Morelia, Mexico City 04510, DF, Mexico.
EM l.rodriguez@crya.unam.mx
RI Faculty of, Sciences, KAU/E-7305-2017
FU DGAPA, UNAM; CONACyT (Mexico); National Aeronautics and Space
   Administration through the NASA Astrobiology Institute [NNA09DA77A]
FX LFR acknowledges the support of DGAPA, UNAM, and of CONACyT (Mexico). BR
   and HFC acknowledge support by the National Aeronautics and Space
   Administration through the NASA Astrobiology Institute under Cooperative
   Agreement No. NNA09DA77A issued through the Office of Space Science.
   This research has made use of the SIMBAD database, operated at CDS,
   Strasbourg, France.
NR 42
TC 0
Z9 0
U1 0
U2 0
PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA
PI MEXICO CITY
PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO
SN 0185-1101
J9 REV MEX ASTRON ASTR
JI Rev. Mex. Astron. Astrofis.
PD OCT
PY 2014
VL 50
IS 2
BP 285
EP 291
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ2YI
UT WOS:000342655500011
ER

PT J
AU Johnson, N
   Naguib, H
   Turner, T
   Anderson, I
   Bassiri-Gharb, N
   Daqaq, M
   Sundaresan, VB
   Sarles, A
AF Johnson, Nancy
   Naguib, Hani
   Turner, Travis
   Anderson, Iain
   Bassiri-Gharb, Nazanin
   Daqaq, Mohammed
   Sundaresan, Vishnu Baba
   Sarles, Andy
TI Adaptive and active materials: selected papers from the ASME 2013
   Conference on Smart Materials, Adaptive Structures and Intelligent
   Systems (SMASIS 13) (Snowbird, UT, USA, 16-18 September 2013)
SO SMART MATERIALS AND STRUCTURES
LA English
DT Editorial Material
C1 [Johnson, Nancy] Gen Motors R&D, Warren, MI 48090 USA.
   [Naguib, Hani] Univ Toronto, Toronto, ON M5S 1A1, Canada.
   [Turner, Travis] NASA, Langley Res Ctr, Hampton, VA USA.
   [Anderson, Iain] Auckland Bioengn Inst, Auckland, New Zealand.
   [Bassiri-Gharb, Nazanin] Georgia Inst Technol, Atlanta, GA 30332 USA.
   [Daqaq, Mohammed] Clemson Univ, Clemson, SC 29631 USA.
   [Sundaresan, Vishnu Baba] Ohio State Univ, Columbus, OH 43210 USA.
RP Johnson, N (reprint author), Gen Motors R&D, Warren, MI 48090 USA.
EM nancy.l.johnson@gm.com
RI Bassiri-Gharb, Nazanin/F-1783-2011
OI Bassiri-Gharb, Nazanin/0000-0002-0183-5160
NR 0
TC 0
Z9 0
U1 2
U2 8
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 2014
VL 23
IS 10
AR 100201
DI 10.1088/0964-1726/23/10/100201
PG 1
WC Instruments & Instrumentation; Materials Science, Multidisciplinary
SC Instruments & Instrumentation; Materials Science
GA AP9AF
UT WOS:000342369900001
ER

PT J
AU Rayman, MD
   Mase, RA
AF Rayman, Marc D.
   Mase, Robert A.
TI Dawn's operations in cruise from Vesta to Ceres
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Dawn; Vesta; Ceres; Asteroid; Ion propulsion; Solar electric propulsion
ID ELECTRIC PROPULSION; MISSION; EXPLORATION
AB On 5 September 2012, Dawn concluded its successful exploration of Vesta, the second most massive object in the main asteroid belt. The spacecraft departed after 14 months in orbit and is now using its ion propulsion system to travel to dwarf planet Ceres, the most massive main-belt asteroid. The principal activity now is thrusting with the ion propulsion system to provide the 3.5 km/s required to rendezvous with Ceres early in 2015. Because two of the four reaction wheels have experienced faults and are likely unrecoverable, a substantial effort has been invested in preparing for Ceres operations with alternate attitude control methods. The project has engaged in an intensive campaign to reduce hydrazine expenditures, which has resulted in a significant increase in the hydrazine expected to be available for Ceres. Based on this work, studies provide good confidence that the required activities at Ceres can be completed. This paper describes post-Vesta operations, including measures taken to conserve hydrazine as well as other preparations for Ceres. (C) 2014 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Rayman, Marc D.; Mase, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Rayman, MD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mrayman@jpl.nasa.gov
NR 12
TC 0
Z9 1
U1 0
U2 6
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 2014
VL 103
BP 113
EP 118
DI 10.1016/j.actaastro.2014.06.042
PG 6
WC Engineering, Aerospace
SC Engineering
GA AP7NX
UT WOS:000342265100011
ER

PT J
AU Thumm, T
   Robinson, JA
   Alleyne, C
   Hasbrook, P
   Mayo, S
   Buckley, N
   Johnson-Green, P
   Karabadzhak, G
   Kamigaichi, S
   Umemura, S
   Sorokin, IV
   Zell, M
   Istasse, E
   Sabbagh, J
   Pignataro, S
AF Thumm, Tracy
   Robinson, Julie A.
   Alleyne, Camille
   Hasbrook, Pete
   Mayo, Susan
   Buckley, Nicole
   Johnson-Green, Perry
   Karabadzhak, George
   Kamigaichi, Shigeki
   Umemura, Sayaka
   Sorokin, Igor V.
   Zell, Martin
   Istasse, Eric
   Sabbagh, Jean
   Pignataro, Salvatore
TI International space station accomplishments update: Scientific
   discovery, advancing future exploration, and benefits brought home to
   earth
SO ACTA ASTRONAUTICA
LA English
DT Article
DE ISS; Research; Microgravity; STEM; Benefits; Utilization
ID BONE
AB Throughout the history of the International Space Station (ISS), crews on board have conducted a variety of scientific research and educational activities. Well into the second year of full utilization of the ISS laboratory, the trend of scientific accomplishments and educational opportunities continues to grow. More than 1500 investigations have been conducted on the ISS since the first module launched in 1998, with over 700 scientific publications. The ISS provides a unique environment for research, international collaboration and educational activities that benefit humankind. This paper will provide an up to date summary of key investigations, facilities, publications, and benefits from ISS research that have developed over the past year. Discoveries in human physiology and nutrition have enabled astronauts to return from ISS with little bone loss, even as scientists seek to better understand the new puzzle of "ocular syndrome" affecting the vision of up to half of astronauts. The geneLAB campaign will unify life sciences investigations to seek genomic, proteomic and metabolomics of the effect of microgravity on life as a whole. Combustion scientists identified a new "cold flame" phenomenon that has the potential to improve models of efficient combustion back on Earth. A significant number of instruments in Earth remote sensing and astrophysics are providing new access to data or nearing completion for launch, making ISS a significant platform for understanding of the Earth system and the universe.
   In addition to multidisciplinary research, the ISS partnership conducts a myriad of student led research investigations and educational activities aimed at increasing student interest in science, technology, engineering and mathematics (STEM). Over the past year, the- ISS partnership compiled new statistics of the educational impact of the ISS on students around the world. More than 43 million students, from kindergarten to graduate school, with more than 28 million teachers located in 49 countries have participated in some aspect of ISS educational activities. These activities include student-developed investigations, education competitions and classroom versions of ISS investigations, participating in ISS investigator experiments, ISS hardware development, educational demonstrations and cultural activities. Through the many inquiry-based educational activities, students and teachers are encouraged to participate in the ISS program thus motivating the next generation of students to pursue careers in STEM. (C) 2014 Published by Elsevier Ltd.
C1 [Thumm, Tracy; Mayo, Susan] Barrios Technol Johnson Space Ctr, Mission & Program Integrat Contract, Houston, TX USA.
   [Robinson, Julie A.; Alleyne, Camille; Hasbrook, Pete] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
   [Buckley, Nicole; Johnson-Green, Perry] Canadian Space Agcy, St Hubert, PQ, Canada.
   [Kamigaichi, Shigeki; Umemura, Sayaka] Japan Aerosp Explorat Agcy JAXA, Ibaraki, Japan.
   [Sorokin, Igor V.] SP Korolev Rocket & Space Corp Energia, Korolev, Russia.
   [Zell, Martin; Istasse, Eric] European Space Agcy, NL-2200 AG Noordwijk, Netherlands.
   [Sabbagh, Jean; Pignataro, Salvatore] Italian Space Agcy ASI, Rome, Italy.
RP Thumm, T (reprint author), 2101 Nasa Pkwy, Houston, TX 77058 USA.
EM tracy.thumm-1@nasa.gov; julie.a.robinson@nasa.gov;
   camille.alleyne@nasa.gov; pete.hasbrook@nasa.gov; susan.mayo@nasa.gov;
   nicole.buckley@asc-csa.gc.ca; perry.johnson-green@asc-csa.gc.ca;
   gfk@tsniimash.ru; kamigaichi.shigeki@jaxa.jp; umemura.sayaka@jaxa.jp;
   igor.v.sorokin@rsce.ru; martin.zell@esa.int; eric.istasse@esa.int;
   jean.sabbagh@asi.it; salvatore.pignataro@asi.it
OI Robinson, Julie/0000-0002-6832-6459
NR 9
TC 0
Z9 0
U1 7
U2 27
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 2014
VL 103
BP 235
EP 242
DI 10.1016/j.actaastro.2014.06.017
PG 8
WC Engineering, Aerospace
SC Engineering
GA AP7NX
UT WOS:000342265100021
ER

PT J
AU Hernandez, S
   Barbee, BW
   Bhaskaran, S
   Getzandanner, K
AF Hernandez, Sonia
   Barbee, Brent W.
   Bhaskaran, Shyam
   Getzandanner, Kenneth
TI Mission opportunities for the flight validation of the kinetic impactor
   concept for asteroid deflection
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Kinetic impact; Asteroid deflection; Mission design
ID SPACECRAFT; DESIGN
AB The kinetic impactor technique for deflecting near-Earth objects (NEOs), whereby a spacecraft is directed to collide with a NEO to alter its orbit via momentum transfer, is one of several proposed methods for defending Earth against hazardous NEOs (asteroids and comets). In this paper we present detailed mission design concepts for a feasible and affordable kinetic impactor flight validation mission deployed to a currently known near-Earth asteroid (NEA). Several filter steps are devised that utilize relevant criteria to optimally balance key parameters, such as approach phase angle, estimated NEA diameter, relative velocity at intercept, and current NEA orbit knowledge, and produce refined lists of the most promising candidate target NEAs. (C) 2014 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Hernandez, Sonia] Univ Texas Austin, Austin, TX 78712 USA.
   [Barbee, Brent W.; Getzandanner, Kenneth] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Bhaskaran, Shyam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hernandez, S (reprint author), Univ Texas Austin, 210 E 24th St, Austin, TX 78712 USA.
EM sonia.hernandez@utexas.edu; brent.w.barbee@nasa.gov;
   shyamkumar.bhaskaran@jpl.nasa.gov; kenneth.getzandanner@nasa.gov
NR 24
TC 2
Z9 2
U1 2
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT-NOV
PY 2014
VL 103
BP 309
EP 321
DI 10.1016/j.actaastro.2014.04.013
PG 13
WC Engineering, Aerospace
SC Engineering
GA AP7NX
UT WOS:000342265100028
ER

PT J
AU Bhaskaran, S
   Kennedy, B
AF Bhaskaran, Shyam
   Kennedy, Brian
TI Closed loop terminal guidance navigation for a kinetic impactor
   spacecraft
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Kinetic impact; Asteroid deflection; Autonomous navigation; Closed loop
   guidance
AB A kinetic impactor spacecraft is a viable method to deflect an asteroid which poses a threat to the Earth. The technology to perform such a deflection has been demonstrated by the Deep Impact (DI) mission, which successfully collided with comet Tempel 1 in July 2005 using an onboard autonomous navigation system, called AutoNav, for the terminal phase of the mission. In this paper, we evaluate the ability of AutoNav to impact a wider range of scenarios that a deflection mission could encounter, varying parameters such as the approach velocity, phase angle, size of the asteroid, and the attitude determination accuracy. In particular, we evaluated the capability of AutoNav to impact 100-300 m size asteroids at speeds between 7.5 and 20 km/s at various phase angles. Using realistic Monte Carlo simulations, we tabulated the probability of success of the deflection as a function of these parameters and find the highest sensitivity to be due to the spacecraft attitude determination error. In addition, we also specifically analyzed the impact probability for a proposed mission (called ISIS) which would send an impactor to the asteroid 1999RQ36. We conclude with some recommendations for future work. (C) 2014 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Bhaskaran, Shyam; Kennedy, Brian] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Outer Planet Nav Grp, Pasadena, CA 91109 USA.
RP Bhaskaran, S (reprint author), CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Outer Planet Nav Grp, MS 264-820,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Shyam.Bhaskaran@jpl.nasa.gov
NR 15
TC 2
Z9 2
U1 0
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD OCT-NOV
PY 2014
VL 103
BP 322
EP 332
DI 10.1016/j.actaastro.2014.02.024
PG 11
WC Engineering, Aerospace
SC Engineering
GA AP7NX
UT WOS:000342265100029
ER

PT J
AU Olmstead, A
   Rigby, JR
   Swinbank, M
   Veilleux, S
AF Olmstead, Alice
   Rigby, Jane R.
   Swinbank, Mark
   Veilleux, Sylvain
TI A MAGNIFIED VIEW OF STAR FORMATION AT z=0.9 FROM TWO LENSED GALAXIES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE dust, extinction; galaxies: high-redshift; galaxies: star formation;
   gravitational lensing: strong
ID SPECTRAL ENERGY-DISTRIBUTIONS; MASS-METALLICITY RELATION;
   HUBBLE-SPACE-TELESCOPE; SMALL-MAGELLANIC-CLOUD; FORMING GALAXIES;
   FORMATION RATES; HIGH-REDSHIFT; H-ALPHA; RESOLVED SPECTROSCOPY; INFRARED
   LUMINOSITY
AB We present new narrowband H alpha imaging from the Hubble Space Telescope of two z = 0.91 galaxies that have been lensed by the foreground galaxy cluster A2390. These data probe spatial scales as small as similar to 0.3 kpc, providing a magnified look at the morphology of star formation at an epoch when the global star formation rate (SFR) was high. However, dust attenuates our spatially resolved SFR indicators, the H alpha and rest-UV emission, and we lack a direct measurement of extinction. Other studies have found that ionized gas in galaxies tends to be roughly 50% more obscured than stars; however, given an unextincted measurement of the SFR we can quantify the relative stellar to nebular extinction and the extinction in H alpha. We infer SFRs from Spitzer and Herschel mid- to far-infrared observations and compare these to integrated H alpha and rest-UV SFRs; this yields stellar to nebular extinction ratios consistent with previous studies. We take advantage of high spatial resolution and contextualize these results in terms of the source-plane morphologies, comparing the distribution of H alpha to that of the rest-frame UV and optical light. In one galaxy, we measure separate SFRs in visually distinct clumps, but can set only a lower limit on the extinction and thus the star formation. Consequently, the data are also consistent with there being an equal amount of extinction along the lines of sight to the ionized gas as to the stars. Future observations in the far-infrared could settle this by mapping out the dust directly.
C1 [Olmstead, Alice; Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
   [Swinbank, Mark] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
   [Veilleux, Sylvain] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
   [Veilleux, Sylvain] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
RP Olmstead, A (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
OI Veilleux, Sylvain/0000-0002-3158-6820
FU NASA, at the NASA Goddard Space Flight Center; Alexander von Humboldt
   Foundation; NASA through a grant from the Space Telescope Science
   Institute [11678]; Association of Universities for Research in
   Astronomy, Inc., under NASA [NAS 5-26555]
FX We thank B. Koester and E. Wuyts for helpful discussions, and J. Richard
   for constructing the lens model. S.V. acknowledges support from NASA
   through a Senior NASA Postdoctoral Program (NPP) award held at the NASA
   Goddard Space Flight Center, and from the Alexander von Humboldt
   Foundation for a "renewed visit" to MPE Garching in 2012. We made use of
   Wright's cosmology calculator, Wright (2006). Support for program #
   11678 was provided by NASA through a grant from the Space Telescope
   Science Institute, which is operated by the Association of Universities
   for Research in Astronomy, Inc., under NASA contract NAS 5-26555.
NR 77
TC 0
Z9 0
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD OCT
PY 2014
VL 148
IS 4
AR 65
DI 10.1088/0004-6256/148/4/65
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP7BU
UT WOS:000342233400007
ER

PT J
AU Sahai, R
   Mack-Crane, GP
AF Sahai, Raghvendra
   Mack-Crane, Galen P.
TI THE ASTROSPHERE OF THE ASYMPTOTIC GIANT BRANCH STAR CIT 6
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE circumstellar matter; stars: AGB and post-AGB; stars: individual (CIT
   6); stars: mass-loss
ID BRIGHT CARBON STARS; BOW SHOCK; CIRCUMSTELLAR ENVELOPES; AGB STARS; LINE
   SURVEY; MILKY-WAY; SHELLS; GAS; SIMULATIONS; BETELGEUSE
AB We have discovered two extended half-ring structures in a far-ultraviolet image taken with the GALEX satellite of the well-known mass-losing carbon star CIT 6 (RW LMi). The northern (southern) ring is brighter (fainter) with a diameter of similar to 15' (similar to 18'). These structures most likely represent the astrosphere resulting from the shock interaction of CIT 6's molecular wind with the warm interstellar medium (ISM), as it moves through the latter. These data provide a direct estimate of the size of CIT 6's circumstellar envelope that is a factor similar to 20 larger than previous estimates based on CO millimeter-wave line data. We find that CIT 6 has been undergoing heavy mass-loss for at least 93,000 yr and the total envelope mass is 0.29 M-circle dot or larger, assuming a constant mass-loss rate of 3.2 x 10(-6) M-circle dot yr(-1). Assuming that the shock front has reached a steady state and CIT 6's motion relative to the ISM is in the sky plane, we measure the termination-shock standoff distance directly from the image and find that CIT 6 is moving at a speed of about greater than or similar to 39 (0.17 cm(-3)/n(ISM)) 1/2 km s(-1) through the ISM around it. However, comparisons with published numerical simulations and analytical modeling shows that CIT 6's forward shock (the northern ring) departs from the parabolic shape expected in steady state. We discuss several possible explanations for this departure.
C1 [Sahai, Raghvendra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Mack-Crane, Galen P.] Occidental Coll, Dept Phys, Los Angeles, CA 90041 USA.
RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA.
EM sahai@jpl.nasa.gov
FU NASA
FX We would like to thank an anonymous referee for detailed comments that
   have helped us improve the discussion in this paper. R.S.'s contribution
   to the research described in this publication was carried out at the Jet
   Propulsion Laboratory, California Institute of Technology, under a
   contract with NASA. R.S. thanks NASA for financial support via a GALEXGO
   award. G.M.C. thanks JPL for a NASA Student Independent Research
   Internship (SIRI).
NR 36
TC 4
Z9 4
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD OCT
PY 2014
VL 148
IS 4
AR 74
DI 10.1088/0004-6256/148/4/74
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP7BU
UT WOS:000342233400016
ER

PT J
AU Schneider, G
   Grady, CA
   Hines, DC
   Stark, CC
   Debes, JH
   Carson, J
   Kuchner, MJ
   Perrin, MD
   Weinberger, AJ
   Wisniewski, JP
   Silverstone, MD
   Jang-Condell, H
   Henning, T
   Woodgate, BE
   Serabyn, E
   Moro-Martin, A
   Tamura, M
   Hinz, PM
   Rodigas, TJ
AF Schneider, Glenn
   Grady, Carol A.
   Hines, Dean C.
   Stark, Christopher C.
   Debes, John H.
   Carson, Joe
   Kuchner, Marc J.
   Perrin, Marshall D.
   Weinberger, Alycia J.
   Wisniewski, John P.
   Silverstone, Murray D.
   Jang-Condell, Hannah
   Henning, Thomas
   Woodgate, Bruce E.
   Serabyn, Eugene
   Moro-Martin, Amaya
   Tamura, Motohide
   Hinz, Phillip M.
   Rodigas, Timothy J.
TI PROBING FOR EXOPLANETS HIDING IN DUSTY DEBRIS DISKS: DISK IMAGING,
   CHARACTERIZATION, AND EXPLORATION WITH HST/STIS MULTI-ROLL CORONAGRAPHY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE methods: observational; planet-disk interactions; stars: individual (HD
   15115, HD 15745, HD 32297, HD 53143, HD 61005, HD 92945, HD 107146, HD
   139664, HD 181327, Au Mic, MP Mus)
ID 4796A CIRCUMSTELLAR DISK; SCATTERED-LIGHT IMAGES; STAR AU-MICROSCOPII;
   SUN-LIKE STARS; T TAURI STAR; HD 32297; BETA-PICTORIS; SOLAR-SYSTEM;
   PLANETARY SYSTEM; OPTICAL-IMAGES
AB Spatially resolved scattered-light images of circumstellar debris in exoplanetary systems constrain the physical properties and orbits of the dust particles in these systems. They also inform on co-orbiting (but unseen) planets, the systemic architectures, and forces perturbing the starlight-scattering circumstellar material. Using Hubble Space Telescope (HST)/Space Telescope Imaging Spectrograph (STIS) broadband optical coronagraphy, we have completed the observational phase of a program to study the spatial distribution of dust in a sample of 10 circumstellar debris systems and 1 "mature" protoplanetrary disk, all with HST pedigree, using point-spread-function-subtracted multi-roll coronagraphy. These observations probe stellocentric distances >= 5 AU for the nearest systems, and simultaneously resolve disk substructures well beyond corresponding to the giant planet and Kuiper Belt regions within our own solar system. They also disclose diffuse very low-surface-brightness dust at larger stellocentric distances. Herein we present new results inclusive of fainter disks such as HD 92945 (F-disk/F-star = 5 x 10(-5)), confirming, and better revealing, the existence of a narrow inner debris ring within a larger diffuse dust disk. Other disks with ring-like substructures and significant asymmetries and complex morphologies include HD 181327, for which we posit a spray of ejecta from a recent massive collision in an exo-Kuiper Belt; HD 61005, suggested to be interacting with the local interstellar medium; and HD 15115 and HD 32297, also discussed in the context of putative environmental interactions. These disks and HD 15745 suggest that debris system evolution cannot be treated in isolation. For AU Mic's edge-on disk, we find out-of-plane surface brightness asymmetries at >= 5 AU that may implicate the existence of one or more planetary perturbers. Time-resolved images of the MP Mus protoplanetary disk provide spatially resolved temporal variability in the disk illumination. These and other new images from our HST/STIS GO/12228 program enable direct inter-comparison of the architectures of these exoplanetary debris systems in the context of our own solar system.
C1 [Schneider, Glenn; Hinz, Phillip M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
   [Schneider, Glenn; Hinz, Phillip M.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
   [Grady, Carol A.] Eureka Sci, Oakland, CA 96002 USA.
   [Hines, Dean C.; Debes, John H.; Perrin, Marshall D.; Moro-Martin, Amaya] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Stark, Christopher C.; Kuchner, Marc J.; Woodgate, Bruce E.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
   [Carson, Joe] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
   [Weinberger, Alycia J.; Rodigas, Timothy J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
   [Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
   [Silverstone, Murray D.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
   [Jang-Condell, Hannah] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
   [Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Tamura, Motohide] Univ Tokyo, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
RP Schneider, G (reprint author), Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
EM gschneider@as.arizona.edu
OI Jang-Condell, Hannah/0000-0002-7639-1322
NR 116
TC 42
Z9 42
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD OCT
PY 2014
VL 148
IS 4
AR 59
DI 10.1088/0004-6256/148/4/59
PG 50
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP7BU
UT WOS:000342233400001
ER

PT J
AU Szkody, P
   Everett, ME
   Howell, SB
   Landolt, AU
   Bond, HE
AF Szkody, Paula
   Everett, Mark E.
   Howell, Steve B.
   Landolt, Arlo U.
   Bond, Howard E.
TI FOLLOW UP OBSERVATIONS OF SDSS AND CRTS CANDIDATE CATACLYSMIC VARIABLES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: close; novae, cataclysmic variables; stars: dwarf novae
ID DIGITAL SKY SURVEY; TIME TRANSIENT SURVEY; HIGH-SPEED PHOTOMETRY; VV
   PUPPIS; SPECTROSCOPY; TARGETS; VIII.
AB We present photometry and spectroscopy of 11 and 35 potential cataclysmic variables, respectively, from the Sloan Digital Sky Survey, the Catalina Real-Time Transient Survey, and vsnet alerts. The photometry results include quasi-periodic oscillations during the decline of V1363 Cyg, nightly accretion changes in the likely Polar (AM Herculis binary) SDSS J1344+20, eclipses in SDSS J2141+05 with an orbital period of 76 +/- 2 minutes, and possible eclipses in SDSS J2158+09 at an orbital period near 100 minutes. Time-resolved spectra reveal short orbital periods near 80 minutes for SDSS J0206+20, 85 minutes for SDSS J1502+33, and near 100 minutes for CSS J0015+26, RXS J0150+37, SDSS J1132+62, SDSS J2154+15, and SDSS J2158+09. The prominent He II line and velocity amplitude of SDSS J2154+15 are consistent with a Polar nature for this object, while the absence of this line and a low velocity amplitude argue against this classification for RXS J0150+37. Single spectra of 10 objects were obtained near outburst and the rest near quiescence, confirming the dwarf novae nature of these objects.
C1 [Szkody, Paula] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
   [Everett, Mark E.] Natl Op Astron Observ, Tucson, AZ 85719 USA.
   [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Landolt, Arlo U.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
   [Bond, Howard E.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Szkody, P (reprint author), Univ Washington, Dept Astron, POB 351580, Seattle, WA 98195 USA.
EM szkody@astro.washington.edu; dsilva@noao.edu; steve.b.howell@nasa.gov;
   landolt@rouge.phys.lsu.edu; heb11@psu.edu
FU NSF [AST-1008734, AST-0803158]; STScI Director's Discretionary Research
   Fund
FX P.S. and S.V.-S. acknowledge support from NSF grant AST-1008734. A.L.
   acknowledges NSF grant AST-0803158. H.E.B. acknowledges the STScI
   Director's Discretionary Research Fund for travel support. All authors
   thank the visionaries who created the National Observatory that served
   the community so well for so many years.
NR 34
TC 5
Z9 5
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD OCT
PY 2014
VL 148
IS 4
AR 63
DI 10.1088/0004-6256/148/4/63
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP7BU
UT WOS:000342233400005
ER

PT J
AU Anderson, DC
   Loughner, CP
   Diskin, G
   Weinheimer, A
   Canty, TP
   Salawitch, RJ
   Worden, HM
   Fried, A
   Mikoviny, T
   Wisthaler, A
   Dickerson, RR
AF Anderson, Daniel C.
   Loughner, Christopher P.
   Diskin, Glenn
   Weinheimer, Andrew
   Canty, Timothy P.
   Salawitch, Ross J.
   Worden, Helen M.
   Fried, Alan
   Mikoviny, Tomas
   Wisthaler, Armin
   Dickerson, Russell R.
TI Measured and modeled CO and NOy in DISCOVER-AQ: An evaluation of
   emissions and chemistry over the eastern US
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Air quality; National Emissions Inventory; CO; NOx; On-road emissions;
   CMAQ
ID REMOTE-SENSING MEASUREMENTS; VEHICLE EMISSIONS; LOS-ANGELES; OZONE;
   CALIFORNIA; TRENDS; BAY
AB Data collected during the 2011 DISCOVER-AQ field campaign in the Baltimore Washington region were used to evaluate CO and NOx emissions in the National Emissions Inventory (NEI). The average emissions ratio for the region was seen to be 11.2 +/- 1.2 mol CO/mol NOx, 21% higher than that predicted by the NEI. Comparisons between in situ and remote observations and CMAQ model output show agreement in CO emissions of 15 +/- 11% while NOx emissions are overestimated by 51-70% in Maryland. Satellite observations of CO by MOPITT show agreement with the Community Multiscale Air Quality (CMAQ) model within 3% over most of the eastern United States. CMAQ NOy mixing ratios were a factor of two higher than observations and result from a combination of errors in emissions and PAN and alkyl nitrate chemistry, as shown by comparison of three CMAQ model runs. Point source NOx emissions are monitored and agree with modeled emissions within 1% on a monthly basis. Because of this accuracy and the NEI assertion that approximately 3/4 of emissions in the Baltimore Washington region are from mobile sources, the MOVES model's treatment of emissions from aging vehicles should be investigated; the NEI overestimate of NOx emissions could indicate that engines produce less NOx and catalytic converters degrade more slowly than assumed by MOVES2010. The recently released 2011 NEI has an even lower CO/NOx emissions ratio than the projection used in this study; it overestimates NOx emissions by an even larger margin. The implications of these findings for US air quality policy are that NOx concentrations near areas of heavy traffic are overestimated and ozone production rates in these locations are slower than models indicate. Results also indicate that ambient ozone concentrations will respond more efficiently to NOx emissions controls but additional sources may need to be targeted for reductions. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Anderson, Daniel C.; Canty, Timothy P.; Salawitch, Ross J.; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
   [Loughner, Christopher P.; Salawitch, Ross J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
   [Loughner, Christopher P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Diskin, Glenn] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Weinheimer, Andrew; Worden, Helen M.] Natl Ctr Atmospher Res, Boulder, CO 80305 USA.
   [Fried, Alan] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80303 USA.
   [Mikoviny, Tomas] Oak Ridge Associated Univ, Oak Ridge, TN 37830 USA.
   [Wisthaler, Armin] Univ Innsbruck, Inst Ionenphys & Angew Phys, A-6020 Innsbruck, Austria.
RP Anderson, DC (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
EM danderson@atmos.umd.edu
RI Salawitch, Ross/B-4605-2009; Anderson, Daniel/I-4398-2014; Dickerson,
   Russell/F-2857-2010; Canty, Timothy/F-2631-2010; 
OI Salawitch, Ross/0000-0001-8597-5832; Anderson,
   Daniel/0000-0002-9826-9811; Dickerson, Russell/0000-0003-0206-3083;
   Canty, Timothy/0000-0003-0618-056X; Loughner,
   Christopher/0000-0002-3833-2014
FU NASA; AQAST
FX We thank Andreas Beyersdorf and Bruce Anderson (NASA Langley) for
   aerosol data, Ron Cohen (UC Berkeley) for TDLIF measurements, and David
   Krask (MDE) for surface isoprene observations. This work was supported
   by grants from NASA and AQAST.
NR 37
TC 18
Z9 18
U1 8
U2 67
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 2014
VL 96
BP 78
EP 87
DI 10.1016/j.atmosenv.2014.07.004
PG 10
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AP7HF
UT WOS:000342247700009
ER

PT J
AU Stavros, EN
   Abatzoglou, JT
   McKenzie, D
   Larkin, NK
AF Stavros, E. Natasha
   Abatzoglou, John T.
   McKenzie, Donald
   Larkin, Narasimhan K.
TI Regional projections of the likelihood of very large wildland fires
   under a changing climate in the contiguous Western United States
SO CLIMATIC CHANGE
LA English
DT Article
ID MEGA-FIRES; WILDFIRE; MODEL; VARIABILITY; ECOSYSTEMS; FORESTS; REGIMES;
   TRENDS; IMPACT
AB Seasonal changes in the climatic potential for very large wildfires (VLWF a parts per thousand yenaEuro parts per thousand 50,000 ac similar to 20,234 ha) across the western contiguous United States are projected over the 21st century using generalized linear models and downscaled climate projections for two representative concentration pathways (RCPs). Significant (p a parts per thousand currency signaEuro parts per thousand 0.05) increases in VLWF probability for climate of the mid-21st century (2031-2060) relative to contemporary climate are found, for both RCP 4.5 and 8.5. The largest differences are in the Eastern Great Basin, Northern Rockies, Pacific Northwest, Rocky Mountains, and Southwest. Changes in seasonality and frequency of VLWFs d7epend on changes in the future climate space. For example, flammability-limited areas such as the Pacific Northwest show that (with high model agreement) the frequency of weeks with VLWFs in a given year is 2-2.7 more likely. However, frequency of weeks with at least one VLWF in fuel-limited systems like the Western Great Basin is 1.3 times more likely (with low model agreement). Thus, areas where fire is directly associated with hot and dry climate, as opposed to experiencing lagged effects from previous years, experience more change in the likelihood of VLWF in future projections. The results provide a quantitative foundation for management to mitigate the effects of VLWFs.
C1 [Stavros, E. Natasha] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Abatzoglou, John T.] Univ Idaho, Dept Geog, Moscow, ID 83843 USA.
   [McKenzie, Donald; Larkin, Narasimhan K.] US Forest Serv, Pacific Wildland Fire Sci Lab, Seattle, WA USA.
RP Stavros, EN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 233-300, Pasadena, CA 91109 USA.
EM natasha.stavros@jpl.nasa.gov
OI Abatzoglou, John/0000-0001-7599-9750
FU Pacific Northwest Research Station, U.S. Forest Service; Joint Fire
   Science Program [11-1-7-4]; National Aeronautics and Space
   Administration
FX The Pacific Northwest Research Station, U.S. Forest Service, and the
   Joint Fire Science Program, project 11-1-7-4, provided funding for this
   paper. The authors would like to thank Robert Norheim, with the
   University of Washington, for designing maps used in the analysis and
   organizing the data, as well as Ernesto Alvarado, Christian Torgersen,
   Tim Essington, David L. Peterson, and Tara Strand for constructive
   reviews. The final stages of this work were carried out at the Jet
   Propulsion Laboratory, California Institute of Technology, under
   contract with the National Aeronautics and Space Administration.
   Copyright 2014. All rights reserved.
NR 41
TC 18
Z9 18
U1 1
U2 50
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0165-0009
EI 1573-1480
J9 CLIMATIC CHANGE
JI Clim. Change
PD OCT
PY 2014
VL 126
IS 3-4
BP 455
EP 468
DI 10.1007/s10584-014-1229-6
PG 14
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AP9VD
UT WOS:000342428000013
ER

PT J
AU Cable, ML
   Horst, SM
   He, C
   Stockton, AM
   Mora, MF
   Tolbert, MA
   Smith, MA
   Willis, PA
AF Cable, M. L.
   Hoerst, S. M.
   He, C.
   Stockton, A. M.
   Mora, M. F.
   Tolbert, M. A.
   Smith, M. A.
   Willis, P. A.
TI Identification of primary amines in Titan tholins using microchip
   nonaqueous capillary electrophoresis
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Titan; microfluidics; ethanol; ethylamine; lab-on-a-chip
ID ORGANIC-CHEMISTRY; UPPER-ATMOSPHERE; EARLY EARTH; PREBIOTIC CHEMISTRY;
   CHEMICAL EVOLUTION; MASS-SPECTROMETRY; AEROSOLS ANALOGS; HAZE;
   HYDROLYSIS; DISCHARGE
AB Titan, the moon of Saturn with a thick atmosphere and an active hydrocarbon-based weather cycle, is considered the best target in the solar system for the study of organic chemistry on a planetary scale. Microfluidic devices that employ liquid phase techniques such as capillary electrophoresis with ultrasensitive laser-induced fluorescence detection offer a unique solution for in situ analysis of complex organics on Titan. We previously reported a protocol for nonaqueous microfluidic analysis of primary aliphatic amines in ethanol, and demonstrated separations of short- and long-chain amines down to -20 degrees C. We have optimized this protocol further, and used it to analyze Titan aerosol analogues (tholins) generated in two separate laboratories under a variety of different conditions. Ethylamine was a major product in all samples, though significant differences in amine content were observed, in particular for long-chain amines (C12-C27). This work validates microfluidic chemical analysis of complex organics with relevance to Titan, and represents a significant first step in understanding tholin composition via targeted functional group analysis. (C) 2014 Published by Elsevier B.V.
C1 [Cable, M. L.; Stockton, A. M.; Mora, M. F.; Willis, P. A.] NASA, Instrument Elect & Sensors Sect, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Hoerst, S. M.; Tolbert, M. A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
   [He, C.; Smith, M. A.] Univ Houston, Dept Chem, Houston, TX 77004 USA.
   [Tolbert, M. A.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
RP Willis, PA (reprint author), NASA, Instrument Elect & Sensors Sect, Jet Prop Lab, Pasadena, CA 91109 USA.
RI Horst, Sarah/A-9906-2010; Mora, Maria/C-9753-2009; Willis,
   Peter/I-6621-2012
OI Horst, Sarah/0000-0003-4596-0702; 
FU NASA Postdoctoral Program (NPP) at the Jet Propulsion Laboratory; NASA
   [NNX11AD82G, NNX12AD92G, NNG05GO58G]; NSF Astronomy and Astrophysics
   Postdoctoral Fellowship [AST-1102827]; NASA Astrobiology Initiative
   through JPL [1372177]; NASA Astrobiology Science and Technology
   Development (ASTID) Program [104320]
FX The authors thank Mike Malaska for helpful discussions, and two
   anonymous reviewers for insightful comments. MLC and AMS were funded
   through the NASA Postdoctoral Program (NPP) at the Jet Propulsion
   Laboratory, administered by the Oak Ridge Associated Universities
   through a contract with NASA. SMH is supported by NSF Astronomy and
   Astrophysics Postdoctoral Fellowship AST-1102827. MAT was funded through
   NASA Exobiology Grant NNX12AD92G and NASA Planetary Atmospheres
   NNX11AD82G. CH and MAS were funded through NASA Exobiology Grant
   NNG05GO58G and the NASA Astrobiology Initiative, through JPL subcontract
   1372177. MFM and PAW were funded through the NASA Astrobiology Science
   and Technology Development (ASTID) Program (Project No. 104320). This
   work was carried out at the Jet Propulsion Laboratory, California
   Institute of Technology, under contract with NASA.
NR 64
TC 10
Z9 10
U1 6
U2 51
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 2014
VL 403
BP 99
EP 107
DI 10.1016/j.epsl.2014.06.028
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP7GZ
UT WOS:000342247100010
ER

PT J
AU Frank, DR
   Zolensky, ME
   Le, L
AF Frank, David R.
   Zolensky, Michael E.
   Le, Loan
TI Olivine in terminal particles of Stardust aerogel tracks and analogous
   grains in chondrite matrix
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID UNEQUILIBRATED ORDINARY CHONDRITES; PORPHYRITIC PYROXENE CHONDRULES;
   INTERPLANETARY DUST PARTICLES; COMET 81P/WILD 2; CARBONACEOUS
   CHONDRITES; AQUEOUS ALTERATION; PLANETARY BASALTS; OXYGEN ISOTOPES;
   SEMARKONA LL3.0; CO3 CHONDRITES
AB The dearth of both major and minor element analyses of anhydrous silicate phases in chondrite matrix has thus far hindered their comparison to the Wild 2 samples. We present 68 analyses of olivine ( Fa(0-97)) in the coarse-grained terminal particles of Stardust aerogel tracks and a comprehensive dataset (>10(3) analyses) of analogous olivine grains ( 5-30 mu m) isolated in CI, CM, CR, CH, CO, CV3-oxidized, CV3-reduced, C3-ungrouped (Acfer 094 and Ningqiang), L/LL 3.0-4, EH3, and Kakangari chondrite matrix. These compositions reveal that Wild 2 likely accreted a diverse assortment of material that was radially transported from various carbonaceous and ordinary chondrite-forming regions. The Wild 2 olivine includes amoeboid olivine aggregates (AOAs), refractory forsterite, type I and type II chondrule fragments and/or microchondrules, and rare relict grain compositions. In addition, we have identified one terminal particle that has no known compositional analog in the meteorite record and may be a signature of low-temperature, aqueous processing in the Kuiper Belt. The generally low Cr content of FeO-rich olivine in the Stardust samples indicates that they underwent mild thermal metamorphism, akin to a petrologic grade of 3.05-3.15. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Frank, David R.; Le, Loan] NASA, ESCG, Johnson Space Ctr, Houston, TX 77058 USA.
   [Zolensky, Michael E.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
RP Frank, DR (reprint author), NASA, ESCG, Johnson Space Ctr, Houston, TX 77058 USA.
EM david.r.frank@nasa.gov
FU NASA Cosmochemistry Program grant
FX We would like to especially thank Adrian Brearley, Don Brownlee, and
   Ryan Ogliore for providing tremendously helpful insight and discussions
   over the three years spanning this project. Mike Weisberg, Rhian Jones,
   and Mutsumi Komatsu also gave us invaluable input. We thank Roger
   Hewins, Neyda Abreu, and two anonymous reviewers for helping us to
   significantly improve the original manuscript. We are also gratefully
   indebted to Keiko Nakamura-Messenger and Graciela Matrajt for preparing
   the TEM grids in the Stardust collection. We were supported by a NASA
   Cosmochemistry Program grant to MEZ.
NR 95
TC 17
Z9 17
U1 0
U2 6
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 OCT 1
PY 2014
VL 142
BP 240
EP 259
DI 10.1016/j.gca.2014.05.037
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AQ2NB
UT WOS:000342622400017
ER

PT J
AU Hui, FK
   Schuette, AJ
   Spiotta, AM
   Yim, J
   Obuchowski, N
   Rasmussen, PA
   Hussain, MS
   Cawley, CM
   Dion, JE
   Tong, FC
AF Hui, Ferdinand K.
   Schuette, A. Jesse
   Spiotta, Alejandro M.
   Yim, John
   Obuchowski, Nancy
   Rasmussen, Peter A.
   Hussain, Mohammed Shazam
   Cawley, C. Michael
   Dion, Jacques E.
   Tong, Frank C.
TI Flexible tip guides and intermediate catheters: two center experience
   and a proposed taxonomy
SO JOURNAL OF NEUROINTERVENTIONAL SURGERY
LA English
DT Review
ID MECHANICAL EMBOLUS REMOVAL; ACUTE ISCHEMIC-STROKE; INTRACRANIAL
   ANEURYSMS; CEREBRAL-ISCHEMIA; DISTAL ACCESS; MERCI TRIAL; THROMBECTOMY;
   SYSTEM; SAFETY; HELPS
AB Background Stable access to target lesions is foundational to endovascular therapy, be it in hemorrhagic or ischemic disease. Continued evolution in access technology has resulted in next generation catheters that afford improved trackability and proximal support.
   Objective Assess safety and patterns of use at two high volume centers, and conceptualize usage patterns.
   Materials and methods A retrospective review of 608 cases in which a 'next generation' catheter was used during 2008-2010 at Cleveland Clinic (Cleveland, Ohio, USA) and throughout 2009-2010 at Emory University Hospital (Atlanta, Georgia, USA) was conducted, and the cases classified by indication. Catheter placement, distal most location, and related complications were recorded and experience summarized. We also reviewed the differences in the catheters and the rationale for catheter selection, as well as relative costs for each approach.
   Results 311 Neuron 053, 166 Neuron 070, 36 distal access catheter (DAC) 3.9 F, 61 DAC 4.3 F, and 34 DAC 5.2 F catheters were deployed. Of these, 459 placements were in the anterior circulation, 130 in the posterior circulation, 11 in the external carotid artery, and eight were used intravenously. Complication rates were 9/131(6.9%) for the DAC catheter group, 16/311 (5.1%) for the Neuron 053 group, and 14/166 (8.4%) for the Neuron 070 group (p=0.37, chi(2) test).
   Conclusions Next generation access catheters possess characteristics that blend qualities of traditional microcatheters and stiff guide catheters. There was no statistically significant difference in complication rates between the various catheter families in this small retrospective review, and the complication rates were similar to historical complication rates.
C1 [Hui, Ferdinand K.; Rasmussen, Peter A.; Hussain, Mohammed Shazam] Cleveland Clin, Cerebrovasc Ctr Neurol Inst, Cleveland, OH 44195 USA.
   [Schuette, A. Jesse] Tripler Army Med Ctr, Dept Neurosurg, Honolulu, HI 96859 USA.
   [Spiotta, Alejandro M.] Med Univ S Carolina, Dept Neurosci, Div Neurosurg, Charleston, SC 29425 USA.
   [Yim, John] NASA, Glenn Res Ctr, Mech & Fluid Syst Div, Cleveland, OH USA.
   [Obuchowski, Nancy] Cleveland Clin, Quantitat Hlth Serv, Cleveland, OH 44106 USA.
   [Cawley, C. Michael; Dion, Jacques E.; Tong, Frank C.] Emory Univ, Dept Radiol, Atlanta, GA 30322 USA.
   [Cawley, C. Michael; Dion, Jacques E.; Tong, Frank C.] Emory Univ, Dept Neurosurg, Atlanta, GA 30322 USA.
RP Hui, FK (reprint author), Cleveland Clin, Cerebrovasc Ctr Neurol Inst, 9500 Euclid Ave,S-80, Cleveland, OH 44195 USA.
EM huif@ccf.org
NR 20
TC 1
Z9 2
U1 0
U2 2
PU BMJ PUBLISHING GROUP
PI LONDON
PA BRITISH MED ASSOC HOUSE, TAVISTOCK SQUARE, LONDON WC1H 9JR, ENGLAND
SN 1759-8478
EI 1759-8486
J9 J NEUROINTERV SURG
JI J. NeuroInterventional Surg.
PD OCT
PY 2014
VL 6
IS 8
BP 618
EP 623
DI 10.1136/neurintsurg-2013-010892
PG 6
WC Neuroimaging; Surgery
SC Neurosciences & Neurology; Surgery
GA AQ1FX
UT WOS:000342528400010
PM 24014468
ER

PT J
AU Tompson, SR
AF Tompson, Sara R.
TI In the Light of Science: Our Ancient Quest for Knowledge and the Measure
   of Modern Physics
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 1
U2 1
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD OCT 1
PY 2014
VL 139
IS 16
BP 107
EP 108
PG 2
WC Information Science & Library Science
SC Information Science & Library Science
GA AQ0OO
UT WOS:000342482800201
ER

PT J
AU Romanski, J
   Romanou, A
   Bauer, M
   Tselioudis, G
AF Romanski, Joy
   Romanou, Anastasia
   Bauer, Michael
   Tselioudis, George
TI Teleconnections, midlatitude cyclones and Aegean Sea turbulent heat flux
   variability on daily through decadal time scales
SO REGIONAL ENVIRONMENTAL CHANGE
LA English
DT Article
DE Aegean; Turbulent flux; Cyclone frequency; Deepwater formation;
   Teleconnections
ID MEDITERRANEAN DEEP WATERS; LABRADOR SEA; THERMOHALINE CIRCULATION;
   INTERANNUAL VARIABILITY; OBJECTIVE CLIMATOLOGY; CONVECTION; WINTER;
   PRECIPITATION; TRENDS; REGION
AB We analyze daily wintertime cyclone variability in the central and eastern Mediterranean during 1958-2001 and identify four distinct "cyclone states," corresponding to the presence or absence of cyclones in each basin. Each cyclone state is associated with wind flows that induce characteristic patterns of cooling via turbulent (sensible and latent) heat fluxes in the eastern Mediterranean basin and Aegean Sea. The relative frequency of occurrence of each state determines the heat loss from the Aegean Sea during that winter, with largest heat losses occurring when there is a storm in the eastern but not central Mediterranean (eNOTc) and the smallest occurring when there is a storm in the central but not eastern Mediterranean (cNOTe). Time series of daily cyclone states for each winter allow us to infer Aegean Sea cooling for winters prior to 1985, the earliest year for which we have daily heat flux observations. We show that cyclone states conducive to Aegean Sea convection occurred in 1991/1992 and 1992/1993, the winters during which deepwater formation was observed in the Aegean Sea, and also during the mid-1970s and the winters of 1963/1964 and 1968/1969. We find that the eNOTc cyclone state is anticorrelated with the North Atlantic Oscillation (NAO) prior to 1977/1978. After 1977/1978, the cNOTe state is anticorrelated with both the NAO and the North Caspian Pattern, showing that the area of influence of large-scale atmospheric teleconnections on regional cyclone activity shifted from the eastern to the central Mediterranean during the late 1970s. A trend toward more frequent occurrence of the positive phase of the NAO produced less frequent cNOTe states since the late 1970s, increasing the number of days with strong cooling of the Aegean Sea surface waters.
C1 [Romanski, Joy] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
   [Romanou, Anastasia; Bauer, Michael] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
   [Tselioudis, George] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Romanski, J (reprint author), Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA.
EM jromanski99@gmail.com
FU NASA [GIT G-35-C56-G1]
FX The authors would like to thank Samuel Somot at Meteo-France, CNRS, and
   Simon Josey at the Ocean Observing and Climate Group, National
   Oceanographic Centre, for their thoughtful discussions, as well as two
   anonymous reviewers, whose comments and suggestions improved this work.
   Funding was provided by the NASA Energy and Water Cycle Study program
   under NASA NEWS Grant GIT G-35-C56-G1. The NAO index was obtained from
   http://www.cpc.ncep.noaa.gov/products/precip/CWlink/pna/nao_index.html
   and the NCP index from
   http://www.cpc.ncep.noaa.gov/products/precip/CWlink/pna/nao_index.html.
NR 51
TC 4
Z9 4
U1 0
U2 5
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1436-3798
EI 1436-378X
J9 REG ENVIRON CHANGE
JI Reg. Envir. Chang.
PD OCT
PY 2014
VL 14
IS 5
SI SI
BP 1713
EP 1723
DI 10.1007/s10113-013-0545-0
PG 11
WC Environmental Sciences; Environmental Studies
SC Environmental Sciences & Ecology
GA AQ0EK
UT WOS:000342455400004
ER

PT J
AU Lupinacci, A
   Kacher, A
   Eilenberg, A
   Shapiro, AA
   Hosemann, P
   Minor, AM
AF Lupinacci, A.
   Kacher, A.
   Eilenberg, A.
   Shapiro, A. A.
   Hosemann, P.
   Minor, A. M.
TI Cryogenic in situ microcompression testing of Sn
SO ACTA MATERIALIA
LA English
DT Article
DE Tin; Solder; DBTT; Small-scale testing; EBSD
ID SOLDER JOINTS; TRANSMISSION EBSD; TIN; BEHAVIOR
AB Characterizing plasticity mechanisms below the ductile-to-brittle transition temperature is traditionally difficult to accomplish in a systematic fashion. Here, we use a new experimental setup to perform in situ cryogenic mechanical testing of pure Sn micropillars at room temperature and at -142 degrees C. Subsequent electron microscopy characterization of the micropillars shows a clear difference in the deformation mechanisms at room temperature and at cryogenic temperatures. At room temperature, the Sn micropillars deformed through dislocation plasticity, while at -142 degrees C they exhibited both higher strength and deformation twinning. Two different orientations were tested, a symmetric (1 0 0) orientation and a non-symmetric (4 (5) over bar 1) orientation. The deformation mechanisms were found to be the same for both orientations. (C) 2014 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Lupinacci, A.; Kacher, A.; Eilenberg, A.; Minor, A. M.] Univ Calif Berkeley, Dept Mat Sci & Engn, Berkeley, CA 94720 USA.
   [Kacher, A.; Minor, A. M.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Natl Ctr Electron Microscopy, Berkeley, CA 94720 USA.
   [Shapiro, A. A.] Jet Prop Lab, Pasadena, CA USA.
   [Hosemann, P.] Univ Calif Berkeley, Dept Nucl Engn, Berkeley, CA 94720 USA.
RP Minor, AM (reprint author), Univ Calif Berkeley, Dept Mat Sci & Engn, Berkeley, CA 94720 USA.
EM aminor@berkeley.edu
RI Foundry, Molecular/G-9968-2014; 
OI Hosemann, Peter/0000-0003-2281-2213
FU NASA GSRP Fellowship; Boeing, Inc.; US Department of Energy
   [DE-AC02-05CH11231]; National Aeronautics and Space Administration
FX Part of this research was carried out at the Jet Propulsion Laboratory,
   California Institute of Technology, under a contract with the National
   Aeronautics and Space Administration. A.L. was supported by a NASA GSRP
   Fellowship and also by Boeing, Inc. We would like to thank both
   Hummingbird Scientific, Inc. and Hysitron, Inc. for help with the design
   and fabrication of the cryogenic testing apparatus. The TEM analysis was
   performed at the National Center for Electron Microscopy at Lawrence
   Berkeley National Laboratory, which is supported by the US Department of
   Energy under Contract No. DE-AC02-05CH11231.
NR 22
TC 8
Z9 8
U1 2
U2 31
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 2014
VL 78
BP 56
EP 64
DI 10.1016/j.actamat.2014.06.026
PG 9
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
   Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA AO7UZ
UT WOS:000341559400006
ER

PT J
AU An, HJ
   Madsen, KK
   Reynolds, SP
   Kaspi, VM
   Harrison, FA
   Boggs, SE
   Christensen, FE
   Craig, WW
   Fryer, CL
   Grefenstette, BW
   Hailey, CJ
   Mori, K
   Stern, D
   Zhang, WW
AF An, Hongjun
   Madsen, Kristin K.
   Reynolds, Stephen P.
   Kaspi, Victoria M.
   Harrison, Fiona A.
   Boggs, Steven E.
   Christensen, Finn E.
   Craig, William W.
   Fryer, Chris L.
   Grefenstette, Brian W.
   Hailey, Charles J.
   Mori, Kaya
   Stern, Daniel
   Zhang, William W.
TI HIGH-ENERGY X-RAY IMAGING OF THE PULSAR WIND NEBULA MSH 15-52:
   CONSTRAINTS ON PARTICLE ACCELERATION AND TRANSPORT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (G320.4-1.2); ISM: jets and outflows; ISM:
   supernova remnants; pulsars: individual (PSR B1509-58); stars: neutron;
   X-rays: ISM
ID CRAB-NEBULA; PSR B1509-58; INTERSTELLAR BUBBLES; MASSIVE STARS;
   EMISSION; EVOLUTION; RADIATION; SPECTRUM; PSR-B1509-58; SPECTROSCOPY
AB We present the first images of the pulsar wind nebula (PWN) MSH 15-52 in the hard X-ray band (greater than or similar to 8 keV), as measured with the Nuclear Spectroscopic Telescope Array (NuSTAR). Overall, the morphology of the PWN as measured by NuSTAR in the 3-7 keV band is similar to that seen in Chandra high-resolution imaging. However, the spatial extent decreases with energy, which we attribute to synchrotron energy losses as the particles move away from the shock. The hard-band maps show a relative deficit of counts in the northern region toward the RCW 89 thermal remnant, with significant asymmetry. We find that the integrated PWN spectra measured with NuSTAR and Chandra suggest that there is a spectral break at 6 keV, which may be explained by a break in the synchrotron-emitting electron distribution at similar to 200 TeV and/or imperfect cross calibration. We also measure spatially resolved spectra, showing that the spectrum of the PWN softens away from the central pulsar B1509-58, and that there exists a roughly sinusoidal variation of spectral hardness in the azimuthal direction. We discuss the results using particle flow models. We find non-monotonic structure in the variation with distance of spectral hardness within 50 '' of the pulsar moving in the jet direction, which may imply particle and magnetic-field compression by magnetic hoop stress as previously suggested for this source. We also present two-dimensional maps of spectral parameters and find an interesting shell-like structure in the N-H map. We discuss possible origins of the shell-like structure and their implications.
C1 [An, Hongjun; Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
   [Madsen, Kristin K.; Harrison, Fiona A.; Grefenstette, Brian W.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
   [Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
   [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
   [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
   [Fryer, Chris L.] Los Alamos Natl Lab, CCS 2, Los Alamos, NM 87545 USA.
   [Hailey, Charles J.; Mori, Kaya] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP An, HJ (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
RI Boggs, Steven/E-4170-2015; 
OI Boggs, Steven/0000-0001-9567-4224; Madsen, Kristin/0000-0003-1252-4891
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; NSERC
   Discovery Grant; Accelerator Supplement; FQRNT Centre de Recherche
   Astrophysique du Quebec; Canadian Institute for Advanced Research
   (CIFAR); Canada Research Chairs Program; Lorne Trottier Chair in
   Astrophysics and Cosmology
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 (NuS-TARDAS) jointly developed
   by the ASI Science Data Center (ASDC, Italy) and the California
   Institute of Technology (USA). V.M.K. acknowledges support from an NSERC
   Discovery Grant and Accelerator Supplement, the FQRNT Centre de
   Recherche Astrophysique du Quebec, an R. Howard Webster Foundation
   Fellowship from the Canadian Institute for Advanced Research (CIFAR),
   the Canada Research Chairs Program and the Lorne Trottier Chair in
   Astrophysics and Cosmology.
NR 51
TC 5
Z9 5
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 OCT 1
PY 2014
VL 793
IS 2
AR 90
DI 10.1088/0004-637X/793/2/90
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP3HD
UT WOS:000341965300021
ER

PT J
AU Chen, JH
   Goldsmith, PF
   Viti, S
   Snell, R
   Lis, DC
   Benz, A
   Bergin, E
   Black, J
   Caselli, P
   Encrenaz, P
   Falgarone, E
   Goicoechea, JR
   Hjalmarson, A
   Hollenbach, D
   Kaufman, M
   Melnick, G
   Neufeld, D
   Pagani, L
   van der Tak, F
   van Dishoeck, E
   Yildiz, UA
AF Chen, Jo-Hsin
   Goldsmith, Paul F.
   Viti, Serena
   Snell, Ronald
   Lis, Dariusz C.
   Benz, Arnold
   Bergin, Edwin
   Black, John
   Caselli, Paola
   Encrenaz, Pierre
   Falgarone, Edith
   Goicoechea, Javier R.
   Hjalmarson, Ake
   Hollenbach, David
   Kaufman, Michael
   Melnick, Gary
   Neufeld, David
   Pagani, Laurent
   van der Tak, Floris
   van Dishoeck, Ewine
   Yildiz, Umut A.
TI HERSCHEL HIFI OBSERVATIONS OF O-2 TOWARD ORION: SPECIAL CONDITIONS FOR
   SHOCK ENHANCED EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: molecules; shock waves
ID INTERSTELLAR MOLECULAR CLOUDS; WAVE-ASTRONOMY-SATELLITE; TEMPORAL
   EVOLUTION; HOT CORE; APERTURE SYNTHESIS; COLOGNE DATABASE;
   STAR-FORMATION; MASSIVE STARS; RHO-OPHIUCHI; LINE SURVEY
AB We report observations of molecular oxygen (O-2) rotational transitions at 487 GHz, 774 GHz, and 1121 GHz toward Orion Peak A. The O-2 lines at 487 GHz and 774 GHz are detected at velocities of 10-12 km s(-1) with line widths similar to 3 km s(-1); however, the transition at 1121 GHz is not detected. The observed line characteristics, combined with the results of earlier observations, suggest that the region responsible for the O-2 emission is similar or equal to 9" (6 x 10(16) cm) in size, and is located close to the H-2 Peak 1 position (where vibrationally excited H-2 emission peaks), and not at Peak A, 23" away. The peak O-2 column density is similar to 1.1 x 10(18) cm(-2). The line velocity is close to that of the 621 GHz water maser emission found in this portion of the Orion Molecular Cloud, and having a shock with velocity vector lying nearly in the plane of the sky is consistent with producing maximum maser gain along the line of sight. The enhanced O-2 abundance compared to that generally found in dense interstellar clouds can be explained by passage of a low-velocity C shock through a clump with preshock density 2 x 10(4) cm(-3), if a reasonable flux of UV radiation is present. The postshock O-2 can explain the emission from the source if its line-of-sight dimension is similar or equal to 10 times larger than its size on the plane of the sky. The special geometry and conditions required may explain why O-2 emission has not been detected in the cores of other massive star-forming molecular clouds.
C1 [Chen, Jo-Hsin; Goldsmith, Paul F.; Yildiz, Umut A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Viti, Serena] UCL, Dept Phys & Astron, London WC1E 6BT, England.
   [Snell, Ronald] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
   [Lis, Dariusz C.] CALTECH, Pasadena, CA 91125 USA.
   [Lis, Dariusz C.] Sorbonne Univ, Univ Paris 06, CNRS, Observ Paris,UMR 8112,LERMA, Paris, France.
   [Benz, Arnold] ETH, Inst Astron, CH-8092 Zurich, Switzerland.
   [Bergin, Edwin] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
   [Black, John; Hjalmarson, Ake] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
   [Caselli, Paola; van Dishoeck, Ewine] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
   [Encrenaz, Pierre; Falgarone, Edith] Observ Paris, UMR8112, CNRS, LRA LERMA, F-75231 Paris 05, France.
   [Encrenaz, Pierre; Falgarone, Edith] Ecole Normale Super, F-75231 Paris 05, France.
   [Goicoechea, Javier R.] Inst Ciencia Mat Madrid ICMM CSIC, E-28049 Madrid, Spain.
   [Hollenbach, David] SETI Inst, Mountain View, CA 94043 USA.
   [Kaufman, Michael] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
   [Melnick, Gary] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Neufeld, David] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
   [Pagani, Laurent] Observ Paris, CNRS, LERMA, F-75014 Paris, France.
   [Pagani, Laurent] Observ Paris, CNRS, UMR8112, F-75014 Paris, France.
   [van der Tak, Floris] SRON, Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands.
   [van der Tak, Floris] Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands.
   [van Dishoeck, Ewine] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Chen, JH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Yildiz, Umut/C-5257-2011; Goldsmith, Paul/H-3159-2016; 
OI Yildiz, Umut/0000-0001-6197-2864; Black, John/0000-0001-7221-7207
FU Spanish MINECO [CSD2009-00038, AYA2009-07304, AYA2012-32032]
FX HIFI has been designed and built by a consortium of institutes and
   university departments from across Europe, Canada, and the United States
   ( NASA) under the leadership of SRON, Netherlands Institute for Space
   Research, Groningen, TheNetherlands, and with major contributions from
   Germany, France, and the US. This work was carried out in part at the
   Jet Propulsion Laboratory, California Institute of Technology. J.R.G.
   thanks the Spanish MINECO for funding support under grants
   CSD2009-00038, AYA2009-07304, and AYA2012-32032. We thank Shiya Wang,
   Nathan Crockett, and the NASA Herschel Science Center Helpdesk for the
   help with the data reduction. We appreciate the help from Justin Neill
   with installing and using XCLASS. We thank Tzu-Cheng Peng for providing
   the CO map used in Figure 1. We thank the anonymous reviewer for a
   number of suggestions that improved the clarity of the paper.
NR 63
TC 9
Z9 9
U1 1
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2014
VL 793
IS 2
AR 111
DI 10.1088/0004-637X/793/2/111
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP3HD
UT WOS:000341965300042
ER

PT J
AU Coley, JB
   Corbet, RHD
   Mukai, K
   Pottschmidt, K
AF Coley, Joel B.
   Corbet, Robin H. D.
   Mukai, Koji
   Pottschmidt, Katja
TI PROBING THE MYSTERIES OF THE X-RAY BINARY 4U 1210-64 WITH ASM, PCA,
   MAXI, BAT, AND SUZAKU
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: individual (4U 1210-64); stars: neutron; X-rays: stars
ID PROPORTIONAL COUNTER ARRAY; CENTAURUS X-3; TIMING-EXPLORER; VELA X-1;
   CATACLYSMIC VARIABLES; INTERSTELLAR-MEDIUM; DUST SCATTERING; IGR
   J16207-5129; LINE EMISSION; STELLAR WIND
AB 4U 1210-64 has been postulated to be a high-mass X-ray binary powered by the Be mechanism. X-ray observations with Suzaku, the ISS Monitor of All-sky X-ray Image (MAXI), and the Rossi X-ray Timing Explorer Proportional Counter Array (PCA) and All Sky Monitor (ASM) provide detailed temporal and spectral information on this poorly understood source. Long-term ASM and MAXI observations show distinct high and low states and the presence of a 6.7101 +/- 0.0005 day modulation, interpreted as the orbital period. Folded light curves reveal a sharp dip, interpreted as an eclipse. To determine the nature of the mass donor, the predicted eclipse half-angle was calculated as a function of inclination angle for several stellar spectral types. The eclipse half-angle is not consistent with a mass donor of spectral type B5 V; however, stars with spectral types B0 V or B0-5 III are possible. The best-fit spectral model consists of a power law with index Gamma = 1.85(-0.05)(+0.04) and a high-energy cutoff at 5.5 +/- 0.2 keV modified by an absorber that fully covers the source as well as partially covering absorption. Emission lines from S XVI K alpha, Fe K alpha, FeXXXV K alpha, and Fe XXVI K alpha were observed in the Suzaku spectra. Out of eclipse, the Fe K alpha line flux was strongly correlated with unabsorbed continuum flux, indicating that the Fe I emission is the result of fluorescence of cold dense material near the compact object. The Fe I feature is not detected during eclipse, further supporting an origin close to the compact object.
C1 [Coley, Joel B.; Corbet, Robin H. D.; Mukai, Koji; Pottschmidt, Katja] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
   [Coley, Joel B.; Corbet, Robin H. D.; Mukai, Koji] NASA, Goddard Space Flight Ctr, CRESST, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
   [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, CRESST, Xray Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
RP Coley, JB (reprint author), Univ Maryland Baltimore Cty, 1000 Hilltop Cir, Baltimore, MD 21250 USA.
EM jcoley1@umbc.edu
RI XRAY, SUZAKU/A-1808-2009
NR 87
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 OCT 1
PY 2014
VL 793
IS 2
AR 77
DI 10.1088/0004-637X/793/2/77
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP3HD
UT WOS:000341965300008
ER

PT J
AU Datta, A
   Schenck, DE
   Burns, JO
   Skillman, SW
   Hallman, EJ
AF Datta, Abhirup
   Schenck, David E.
   Burns, Jack O.
   Skillman, Samuel W.
   Hallman, Eric J.
TI HOW MUCH CAN WE LEARN FROM A MERGING COLD FRONT CLUSTER? INSIGHTS FROM
   X-RAY TEMPERATURE AND RADIO MAPS OF A3667
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: abundances; galaxies: clusters: general; radiation mechanisms:
   non-thermal; radiation mechanisms: thermal; X-rays: galaxies: clusters
ID ADAPTIVE MESH REFINEMENT; COOL-CORE CLUSTER; MAGNETIC-FIELD
   AMPLIFICATION; DIFFUSIVE SHOCK ACCELERATION; DEEP CHANDRA OBSERVATION;
   LARGE-SCALE STRUCTURE; GALAXY CLUSTERS; ABELL 3667; XMM-NEWTON;
   COSMOLOGICAL SIMULATIONS
AB The galaxy cluster A3667 is an ideal laboratory to study the plasma processes in the intracluster medium. High-resolution Chandra X-ray observations show a cold front in A3667. At radio wavelengths, A3667 reveals a double radio-relic feature in the outskirts of the cluster. These suggest multiple merger events in this cluster. In this paper, we analyze the substantial archival X-ray observations of A3667 from the Chandra X-ray Observatory and compare these with existing radio observations as well as state-of-the-art adaptive mesh refinement MHD cosmological simulations using Enzo. We have used two temperature map making techniques, weighted Voronoi tessellation and adaptive circular binning, to produce the high-resolution and largest field-of-view temperature maps of A3667. These high-fidelity temperature maps allow us to study the X-ray shocks in the cluster using a new two-dimensional shock-finding algorithm. We have also estimated the Mach numbers from the shocks inferred from previous ATCA radio observations. The combined shock statistics from the X-ray and radio data are in agreement with the shock statistics in a simulated MHD cluster. We have also studied the profiles of the thermodynamic properties across the cold front using similar to 447 ks from the combined Chandra observations on A3667. Our results show that the stability of the cold front in A3667 can be attributed to the suppression of the thermal conduction across the cold front by a factor of similar to 100-700 compared to the classical Spitzer value.
C1 [Datta, Abhirup; Schenck, David E.; Burns, Jack O.; Skillman, Samuel W.; Hallman, Eric J.] Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
   [Datta, Abhirup; Burns, Jack O.] Lunar Univ, Network Astrophys Res LUNAR, NASA Lunar Sci Inst, NASA Ames Res Ctr, Moffett Field, CA 94089 USA.
   [Hallman, Eric J.] Tech X Corp, Boulder, CO 80303 USA.
RP Datta, A (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
EM Abhirup.Datta@colorado.edu
FU NASA Lunar Science Institute; National Science Foundation (NSF) [AST
   1106437]; NSF [CNS-0821794]; University of Colorado, Boulder; NASA Lunar
   Science Institute [NNA09DB30A]
FX We thank Matt Owers for providing the exact locations of the optical
   substructures (shown in Figure 1) and Huub Rottgering for providing the
   FITS images of A3667 from ATCA observations. We also thank Hao Xu for
   the original MHD cluster from Xu et al. (2011) that has been used in
   Skillman et al. (2013) and further used to compare with the A3667
   results in this work. A.D. has been supported by the NASA Postdoctoral
   Fellowship Program through the NASA Lunar Science Institute. This work
   was funded by the National Science Foundation (NSF) grant AST 1106437 to
   J.O.B. This work utilized the Janus supercomputer, which is supported by
   the NSF (award number 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. The LUNAR Consortium
   (http://lunar.colorado.edu), headquartered at the University of
   Colorado, is funded by the NASA Lunar Science Institute (via cooperative
   Agreement NNA09DB30A), and partially supported this research.
NR 104
TC 4
Z9 4
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2014
VL 793
IS 2
AR 80
DI 10.1088/0004-637X/793/2/80
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP3HD
UT WOS:000341965300011
ER

PT J
AU Kalapotharakos, C
   Harding, AK
   Kazanas, D
AF Kalapotharakos, Constantinos
   Harding, Alice K.
   Kazanas, Demosthenes
TI GAMMA-RAY EMISSION IN DISSIPATIVE PULSAR MAGNETOSPHERES: FROM THEORY TO
   FERMI OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: stars; pulsars: general; stars: neutron
ID FORCE-FREE MAGNETOSPHERE; PERFECTLY MATCHED LAYER; NEUTRON-STARS; LIGHT
   CURVES; ELECTROMAGNETIC-WAVES; OBLIQUE ROTATORS; MAGNETIC-FIELD;
   SIMULATIONS; RADIATION; RADIO
AB We compute the patterns of gamma-ray emission due to curvature radiation in dissipative pulsar magnetospheres. Our ultimate goal is to construct macrophysical models that are able to reproduce the observed gamma-ray light curve phenomenology recently published in the Second Fermi Pulsar Catalog. We apply specific forms of Ohm's law on the open field lines using a broad range for the macroscopic conductivity values that result in solutions ranging, from near-vacuum to near-force-free. Using these solutions, we generate model gamma-ray light curves by calculating realistic trajectories and Lorentz factors of radiating particles under the influence of both the accelerating electric fields and curvature radiation reaction. We further constrain our models using the observed dependence of the phase lags between the radio and gamma-ray emission on the gamma-ray peak separation. We perform a statistical comparison of our model radio-lag versus peak-separation diagram and the one obtained for the Fermi standard pulsars. We find that for models of uniform conductivity over the entire open magnetic field line region, agreement with observations favors higher values of this parameter. We find, however, significant improvement in fitting the data with models that employ a hybrid form of conductivity, specifically, infinite conductivity interior to the light cylinder and high but finite conductivity on the outside. In these models the gamma-ray emission is produced in regions near the equatorial current sheet but modulated by the local physical properties. These models have radio lags near the observed values and statistically best reproduce the observed light curve phenomenology. Additionally, they also produce GeV photon cut-off energies.
C1 [Kalapotharakos, Constantinos] Univ Maryland, College Pk, MD 20742 USA.
   [Kalapotharakos, Constantinos; Harding, Alice K.; Kazanas, Demosthenes] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Kalapotharakos, C (reprint author), Univ Maryland, Coll Pk UMDCP CRESST, College Pk, MD 20742 USA.
EM constantinos.kalapotharakos@nasa.gov
FU NASA Astrophysics Theory; Fermi Guest Investigator Programs
FX We would like to thank an anonymous referee for helpful suggestions that
   improved the paper and acknowledge support from the NASA Astrophysics
   Theory and Fermi Guest Investigator Programs. We also thank NASA's
   High-End Computing Program for allotment of time on its supercomputers.
NR 45
TC 23
Z9 23
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 OCT 1
PY 2014
VL 793
IS 2
AR 97
DI 10.1088/0004-637X/793/2/97
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP3HD
UT WOS:000341965300028
ER

PT J
AU Milligan, RO
   Kerr, GS
   Dennis, BR
   Hudson, HS
   Fletcher, L
   Allred, JC
   Chamberlin, PC
   Ireland, J
   Mathioudakis, M
   Keenan, FP
AF Milligan, Ryan O.
   Kerr, Graham S.
   Dennis, Brian R.
   Hudson, Hugh S.
   Fletcher, Lyndsay
   Allred, Joel C.
   Chamberlin, Phillip C.
   Ireland, Jack
   Mathioudakis, Mihalis
   Keenan, Francis P.
TI THE RADIATED ENERGY BUDGET OF CHROMOSPHERIC PLASMA IN A MAJOR SOLAR
   FLARE DEDUCED FROM MULTI-WAVELENGTH OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: chromosphere; Sun: flares; Sun: UV radiation; Sun: X-rays, gamma
   rays
ID WHITE-LIGHT FLARES; IMAGING SPECTROMETER; SPECTROSCOPIC-IMAGER; OPTICAL
   TELESCOPE; MAGNETIC-FIELD; EMISSION; MODEL; IRRADIANCE; SDO/EVE; HINODE
AB This paper presents measurements of the energy radiated by the lower solar atmosphere, at optical, UV, and EUV wavelengths, during an X-class solar flare (SOL2011-02-15T01:56) in response to an injection of energy assumed to be in the form of nonthermal electrons. Hard X-ray observations from RHESSI were used to track the evolution of the parameters of the nonthermal electron distribution to reveal the total power contained in flare accelerated electrons. By integrating over the duration of the impulsive phase, the total energy contained in the nonthermal electrons was found to be >2 x 10(31) erg. The response of the lower solar atmosphere was measured in the free-bound EUV continua of H I (Lyman), He I, and He II, plus the emission lines of He II at 304 angstrom and H I (Ly alpha) at 1216 angstrom by SDO/EVE, the UV continua at 1600 angstrom and 1700 angstrom by SDO/AIA, and the white light continuum at 4504 angstrom, 5550 angstrom, and 6684 angstrom, along with the Ca II H line at 3968 angstrom using Hinode/SOT. The summed energy detected by these instruments amounted to similar to 3 x 10(30) erg; about 15% of the total nonthermal energy. The Ly alpha line was found to dominate the measured radiative losses. Parameters of both the driving electron distribution and the resulting chromospheric response are presented in detail to encourage the numerical modeling of flare heating for this event, to determine the depth of the solar atmosphere at which these line and continuum processes originate, and the mechanism(s) responsible for their generation.
C1 [Milligan, Ryan O.; Mathioudakis, Mihalis; Keenan, Francis P.] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
   [Milligan, Ryan O.; Dennis, Brian R.; Allred, Joel C.; Chamberlin, Phillip C.; Ireland, Jack] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Solar Phys Lab, Greenbelt, MD 20771 USA.
   [Milligan, Ryan O.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
   [Kerr, Graham S.; Hudson, Hugh S.; Fletcher, Lyndsay] Univ Glasgow, Sch Phys & Astron, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
   [Hudson, Hugh S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Ireland, Jack] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Solar Phys Lab,Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Milligan, RO (reprint author), Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland.
EM r.milligan@qub.ac.uk
RI Kerr, Graham /B-2786-2014; Chamberlin, Phillip/C-9531-2012; 
OI Kerr, Graham /0000-0002-5632-2039; Chamberlin,
   Phillip/0000-0003-4372-7405; Hudson, Hugh/0000-0001-5685-1283
FU Leverhulme Trust [F/00203/X]; NASA for LWS/TRT [NNX11AQ53G]; LWS/SDO
   Data Analysis [NNX14AE07G]; College of Science and Engineering at the
   University of Glasgow; NASA for RHESSI [5-98033]; UK's Science &
   Technology Facilities council [ST/I001801, ST/L000741]; European
   Community's Seventh Framework Programme (FP7) [606862]
FX This research was a result of several stimulating discussions between
   participants at a meeting on Chromospheric Flares held at the
   International Space Science Institute (ISSI) in Bern, Switzerland.
   R.O.M. is grateful to the Leverhulme Trust for financial support from
   grant F/00203/X, and to NASA for LWS/TR&T grant NNX11AQ53G and LWS/SDO
   Data Analysis grant NNX14AE07G. G.S.K. acknowledges financial support of
   a postgraduate research scholarship from the College of Science and
   Engineering at the University of Glasgow. H.S.H. thanks NASA for support
   under contract NAS 5-98033 for RHESSI. L.F. acknowledges support from
   the UK's Science & Technology Facilities council (ST/I001801 and
   ST/L000741). The research leading to these results has received funding
   from the European Community's Seventh Framework Programme
   (FP7/2007-2013) under grant agreement no. 606862 (F-CHROMA).
NR 52
TC 31
Z9 31
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 OCT 1
PY 2014
VL 793
IS 2
AR 70
DI 10.1088/0004-637X/793/2/70
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP3HD
UT WOS:000341965300001
ER

PT J
AU Mori, K
   Gotthelf, EV
   Dufour, F
   Kaspi, VM
   Halpern, JP
   Beloborodov, AM
   An, H
   Bachetti, M
   Boggs, SE
   Christensen, FE
   Craig, WW
   Hailey, CJ
   Harrison, FA
   Kouveliotou, C
   Pivovaroff, MJ
   Stern, D
   Zhang, WW
AF Mori, Kaya
   Gotthelf, Eric V.
   Dufour, Francois
   Kaspi, Victoria M.
   Halpern, Jules P.
   Beloborodov, Andrei M.
   An, Hongjun
   Bachetti, Matteo
   Boggs, Steven E.
   Christensen, Finn E.
   Craig, William W.
   Hailey, Charles J.
   Harrison, Fiona A.
   Kouveliotou, Chryssa
   Pivovaroff, Michael J.
   Stern, Daniel
   Zhang, William W.
TI A BROADBAND X-RAY STUDY OF THE GEMINGA PULSAR WITH NuSTAR AND XMM-NEWTON
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE X-rays: individual (Geminga)
ID HIGH-ENERGY; WIND NEBULA; INTERSTELLAR-MEDIUM; TIMING ACCURACY;
   NEUTRON-STARS; PSR B0656+14; RADIATION; EMISSION; SPECTROSCOPY;
   TELESCOPE
AB We report on the first hard X-ray detection of the Geminga pulsar above 10 keV using a 150 ks observation with the Nuclear Spectroscopic Telescope Array (NuSTAR) observatory. The double-peaked pulse profile of non-thermal emission seen in the soft X-ray band persists at higher energies. Broadband phase-integrated spectra over the 0.2-20 keV band with NuSTAR and archival XMM-Newton data do not fit to a conventional two-component model of a blackbody plus power law, but instead exhibit spectral hardening above similar to 5 keV. We find that two spectral models fit the data well: (1) a blackbody (kT(1) similar to 42 eV) with a broken power law (Gamma(1) similar to 2.0, Gamma(2) similar to 1.4 and E-break similar to 3.4 keV) and (2) two blackbody components (kT(1) similar to 44 eV and kT(2) similar to 195 eV) with a power-law component (Gamma similar to 1.7). In both cases, the extrapolation of the Rayleigh-Jeans tail of the thermal component is consistent with the UV data, while the non-thermal component overpredicts the near-infrared data, requiring a spectral flattening at E similar to 0.05-0.5 keV. While strong phase variation of the power-law index is present below similar to 5 keV, our phase-resolved spectroscopy with NuSTAR indicates that another hard non-thermal component with Gamma similar to 1.3 emerges above similar to 5 keV. The spectral hardening in non-thermal X-ray emission as well as spectral flattening between the optical and X-ray bands argue against the conjecture that a single power law may account for multi-wavelength non-thermal spectra of middle-aged pulsars.
C1 [Mori, Kaya; Gotthelf, Eric V.; Halpern, Jules P.; Beloborodov, Andrei M.; Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Dufour, Francois; Kaspi, Victoria M.; An, Hongjun] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
   [Bachetti, Matteo] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
   [Bachetti, Matteo] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France.
   [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
   [Harrison, Fiona A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
   [Kouveliotou, Chryssa] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
   [Pivovaroff, Michael J.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
   [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Mori, K (reprint author), Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
EM kaya@astro.columbia.edu
RI Pivovaroff, Michael/M-7998-2014; Boggs, Steven/E-4170-2015; 
OI Pivovaroff, Michael/0000-0001-6780-6816; Boggs,
   Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337
FU NASA [NNG08FD60C, NNX10AI72G, NNX13AI34G]; NASA/Fermi [NNX12AO89G];
   NASA/Chandra [G03-14066X]; NSERC; FQRNT Centre de Recherche
   Astrophysique du Quebec; Canadian Institute for Advanced Research
   (CIFAR); Canada Research Chairs Program; Lorne Trottier Chair in
   Astrophysics and Cosmology
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). E.V.G. acknowledges support from
   NASA/Fermi grant NNX12AO89G and NASA/Chandra grant G03-14066X. V.M.K.
   acknowledges support from an NSERC Discovery Grant, the FQRNT Centre de
   Recherche Astrophysique du Quebec, an R. Howard Webster Foundation
   Fellowship from the Canadian Institute for Advanced Research (CIFAR),
   the Canada Research Chairs Program, and the Lorne Trottier Chair in
   Astrophysics and Cosmology. A.M.B. acknowledges the support by NASA
   grants NNX10AI72G and NNX13AI34G.
NR 46
TC 5
Z9 5
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 OCT 1
PY 2014
VL 793
IS 2
AR 88
DI 10.1088/0004-637X/793/2/88
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP3HD
UT WOS:000341965300019
ER

PT J
AU Nuevo, M
   Materese, CK
   Sandford, SA
AF Nuevo, Michel
   Materese, Christopher K.
   Sandford, Scott A.
TI THE PHOTOCHEMISTRY OF PYRIMIDINE IN REALISTIC ASTROPHYSICAL ICES AND THE
   PRODUCTION OF NUCLEOBASES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; astrochemistry; ISM: molecules; methods: laboratory:
   molecular; molecular processes; ultraviolet: ISM
ID POLYCYCLIC AROMATIC-HYDROCARBONS; INTERSTELLAR ICE; UV-IRRADIATION;
   ULTRAVIOLET PHOTOIRRADIATION; NITROGEN-HETEROCYCLES; MURCHISON
   METEORITE; ORGANIC RESIDUES; AMINO-ACIDS; EXTRATERRESTRIAL NUCLEOBASES;
   CARBONACEOUS METEORITES
AB Nucleobases, together with deoxyribose/ribose and phosphoric acid, are the building blocks of DNA and RNA for all known life. The presence of nucleobase-like compounds in carbonaceous chondrites delivered to the Earth raises the question of an extraterrestrial origin for the molecules that triggered life on our planet. Whether these molecules are formed in interstellar/protostellar environments, in small parent bodies in the solar system, or both, is currently unclear. Recent experiments show that the UV irradiation of pyrimidine (C4H4N2) in H2O-rich ice mixtures that contain NH3, CH3OH, or CH4 leads to the formation of the pyrimidine-based nucleobases uracil, cytosine, and thymine. In this work, we discuss the low-temperature UV irradiation of pyrimidine in realistic astrophysical ice mixtures containing H2O, CH3OH, and NH3, with or without CH4, to search for the production of nucleobases and other prebiotic compounds. These experiments show the presence of uracil, urea, glycerol, hexamethylenetetramine, small amino acids, and small carboxylic acids in all samples. Cytosine was only found in one sample produced from ices irradiated with a higher UV dose, while thymine was not found in any sample, even after irradiation with a higher UV dose. Results are discussed to evaluate the role of the photochemistry of pyrimidine in the inventory of organic molecules detected in meteorites and their astrophysical/astrobiological implications.
C1 [Nuevo, Michel; Materese, Christopher K.; Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Nuevo, Michel] BAER Inst, Petaluma, CA 94952 USA.
   [Materese, Christopher K.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
RP Nuevo, M (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA.
EM michel.nuevo-1@nasa.gov
FU NASA's Origins of Solar Systems program
FX M.N. and S.A.S. acknowledge NASA's Origins of Solar Systems program for
   financial support. C.K.M. acknowledges the NASA Postdoctoral Program
   administered by ORAU. All authors acknowledge R.L. Walker for technical
   support. Finally, we would like to thank an anonymous reviewer for
   useful comments and suggestions.
NR 55
TC 13
Z9 13
U1 2
U2 33
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 OCT 1
PY 2014
VL 793
IS 2
AR 125
DI 10.1088/0004-637X/793/2/125
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP3HD
UT WOS:000341965300056
ER

PT J
AU Pucci, S
   Poletto, G
   Sterling, AC
   Romoli, M
AF Pucci, Stefano
   Poletto, Giannina
   Sterling, Alphonse C.
   Romoli, Marco
TI BIRTH, LIFE, AND DEATH OF A SOLAR CORONAL PLUME
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: corona; Sun: UV radiation; techniques: spectroscopic
ID POLAR PLUMES; BRIGHT POINTS; ULYSSES OBSERVATIONS; WIND; EUV; HOLE;
   DISTURBANCES; SPECTROMETER; DYNAMICS; PLASMA
AB We analyze a solar polar-coronal-hole (CH) plume over its entire approximate to 40 hr lifetime, using high-resolution Solar Dynamic Observatory Atmospheric Imaging Assembly (AIA) data. We examine (1) the plume's relationship to a bright point (BP) that persists at its base, (2) plume outflows and their possible contribution to the solar wind mass supply, and (3) the physical properties of the plume. We find that the plume started approximate to 2 hr after the BP first appeared and became undetectable approximate to 1 hr after the BP disappeared. We detected radially moving radiance variations from both the plume and from interplume regions, corresponding to apparent outflow speeds ranging over approximate to(30-300) km s(-1) with outflow velocities being higher in the "cooler" AIA 171 angstrom channel than in the "hotter" 193 angstrom and 211 angstrom channels, which is inconsistent with wave motions; therefore, we conclude that the observed radiance variations represent material outflows. If they persist into the heliosphere and plumes cover approximate to 10% of a typical CH area, these flows could account for approximate to 50% of the solar wind mass. From a differential emission measure analysis of the AIA images, we find that the average electron temperature of the plume remained approximately constant over its lifetime, at T-e approximate to 8.5 x 10(5) K. Its density, however, decreased with the age of the plume, being about a factor of three lower when the plume faded compared to when it was born. We conclude that the plume died due to a density reduction rather than to a temperature decrease.
C1 [Pucci, Stefano; Romoli, Marco] Univ Florence, Dept Phys & Astron, I-50125 Florence, Italy.
   [Poletto, Giannina] INAF Arcetri Astrophys Observ, I-50125 Florence, Italy.
   [Sterling, Alphonse C.] NASA MSFC, Space Sci Off, Huntsville, AL 35812 USA.
RP Pucci, S (reprint author), Univ Florence, Dept Phys & Astron, Largo Enrico Fermi 5, I-50125 Florence, Italy.
EM stpucci@arcetri.astro.it
RI Romoli, Marco/H-6859-2012
FU ASI [I/023/09/0]; NASA's Office of Space Science
FX S.P. and G.P. acknowledge support from ASI I/023/09/0. A.C.S. was
   supported by funding from NASA's Office of Space Science through the
   Living With a Star Targeted Research & Technology Program. A.C.S. also
   benefited from discussions held at the International Space Science
   Institute's (ISSI, Bern, Switzerland) International Team on Solar
   Coronal Jets.
NR 30
TC 5
Z9 5
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 OCT 1
PY 2014
VL 793
IS 2
AR 86
DI 10.1088/0004-637X/793/2/86
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP3HD
UT WOS:000341965300017
ER

PT J
AU Summerlin, EJ
   Vinas, AF
   Moore, TE
   Christian, ER
   Cooper, JF
AF Summerlin, Errol J.
   Vinas, Adolfo F.
   Moore, Thomas E.
   Christian, Eric R.
   Cooper, John F.
TI ON THE STABILITY OF PICK-UP ION RING DISTRIBUTIONS IN THE OUTER
   HELIOSHEATH
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: general; plasmas; scattering; solar wind; Sun: heliosphere; waves
ID INTERSTELLAR MAGNETIC-FIELD; BOUNDARY EXPLORER IBEX; SOLAR-SYSTEM;
   INSTABILITIES; RIBBON; ENVIRONMENT
AB The "secondary energetic neutral atom (ENA)" hypothesis for the ribbon feature observed by the Interstellar Boundary Explorer (IBEX) posits that the neutral component of the solar wind continues beyond the heliopause and charge exchanges with interstellar ions in the Outer Heliosheath (OHS). This creates pick-up ions that gyrate about the draped interstellar magnetic field (ISMF) lines at pitch angles near 90 degrees. on the locus where the ISMF lies tangential to the heliopause and perpendicular to the heliocentric radial direction. This location closely coincides with the location of the ribbon feature according to the prevailing inferences of the ISMF orientation and draping. The locally gyrating ions undergo additional charge exchange and escape as free-flying neutral atoms, many of which travel back toward the inner solar system and are imaged by IBEX as a ribbon tracing out the locus described above. For this mechanism to succeed, the pick-up ions must diffuse in pitch angle slowly enough to permit secondary charge exchange before their pitch angle distribution substantially broadens away from 90 degrees. Previous work using linear Vlasov dispersion analysis of parallel propagating waves has suggested that the ring distribution in the OHS is highly unstable, which, if true, would make the secondary ENA hypothesis incapable of rendering the observed ribbon. In this paper, we extend this earlier work to more realistic ring distribution functions. We find that, at the low densities necessary to produce the observed IBEX ribbon via the secondary ENA hypothesis, growth rates are highly sensitive to the temperature of the beam and that even very modest temperatures of the ring beam corresponding to beam widths of <1 degrees. are sufficient to damp the self-generated waves associated with the ring beam. Thus, at least from the perspective of linear Vlasov dispersion analysis of parallel propagating waves, there is no reason to expect that the ring distributions necessary to produce the observed IBEX ENA flux via the secondary ENA hypothesis will be unstable to their own self-generated turbulence.
C1 [Summerlin, Errol J.; Vinas, Adolfo F.; Moore, Thomas E.; Christian, Eric R.; Cooper, John F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Summerlin, EJ (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM errol.summerlin@nasa.gov; adolfo.figueroa-vinas-1@nasa.gov;
   thomas.e.moore@nasa.gov; eric.r.christian@nasa.gov;
   john.f.cooper@nasa.gov
NR 16
TC 6
Z9 6
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 OCT 1
PY 2014
VL 793
IS 2
AR 93
DI 10.1088/0004-637X/793/2/93
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP3HD
UT WOS:000341965300024
ER

PT J
AU Switzer, ER
   Liu, A
AF Switzer, Eric R.
   Liu, Adrian
TI ERASING THE VARIABLE: EMPIRICAL FOREGROUND DISCOVERY FOR GLOBAL 21 cm
   SPECTRUM EXPERIMENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark ages, reionization, first stars; methods: data analysis; methods:
   statistical
ID GALACTIC RADIO-EMISSION; POWER SPECTRUM; INTERGALACTIC MEDIUM;
   DARK-AGES; TO 0.8; REIONIZATION; EPOCH; MHZ; FREQUENCIES; BRIGHTNESS
AB Spectral measurements of the 21 cm monopole background have the promise of revealing the bulk energetic properties and ionization state of our universe from z similar to 6-30. Synchrotron foregrounds are orders of magnitude larger than the cosmological signal and are the principal challenge faced by these experiments. While synchrotron radiation is thought to be spectrally smooth and described by relatively few degrees of freedom, the instrumental response to bright foregrounds may be much more complex. To deal with such complexities, we develop an approach that discovers contaminated spectral modes using spatial fluctuations of the measured data. This approach exploits the fact that foregrounds vary across the sky while the signal does not. The discovered modes are projected out of each line of sight of a data cube. An angular weighting then optimizes the cosmological signal amplitude estimate by giving preference to lower-noise regions. Using this method, we show that it is essential for the passband to be stable to at least similar to 10(-4). In contrast, the constraints on the spectral smoothness of the absolute calibration are mainly aesthetic if one is able to take advantage of spatial information. To the extent it is understood, controlling polarization to intensity leakage at the similar to 10(-2) level will also be essential to rejecting Faraday rotation of the polarized synchrotron emission.
C1 [Switzer, Eric R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
   [Liu, Adrian] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Liu, Adrian] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
RP Switzer, ER (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM eric.r.switzer@nasa.gov
FU NSF [AST-0804508, AST-1129258, AST-1125558]
FX E.S. thanks Ue-Li Pen for conversations and feedback, and for
   stimulating the approach in collaboration on z similar to 1 21 cm data
   analysis from the Green Bank Telescope. A.L. thanks Matt McQuinn for
   conversations. We thank Harish Vedantham for comments and the Ohio 21 cm
   workshop for fostering conversations that initiated the project. A.L.
   acknowledges support from NSF grants AST-0804508, AST-1129258, and
   AST-1125558.
NR 45
TC 12
Z9 12
U1 0
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 OCT 1
PY 2014
VL 793
IS 2
AR UNSP 102
DI 10.1088/0004-637X/793/2/102
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP3HD
UT WOS:000341965300033
ER

PT J
AU Uzgil, BD
   Aguirre, JE
   Bradford, CM
   Lidz, A
AF Uzgil, B. D.
   Aguirre, J. E.
   Bradford, C. M.
   Lidz, A.
TI MEASURING GALAXY CLUSTERING AND THE EVOLUTION OF [CII] MEAN INTENSITY
   WITH FAR-IR LINE INTENSITY MAPPING DURING 0.5 < z < 1.5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: ISM; infrared: ISM; large-scale structure
   of universe
ID SPACE-OBSERVATORY MEASUREMENTS; STAR-FORMING GALAXIES; C II; INFRARED
   LINE; PHYSICAL CONDITIONS; EARLY UNIVERSE; MOLECULAR GAS; REIONIZATION;
   EMISSION; SPECTROSCOPY
AB Infrared fine-structure emission lines from trace metals are powerful diagnostics of the interstellar medium in galaxies. We explore the possibility of studying the redshifted far-IR fine-structure line emission using the three-dimensional (3D) power spectra obtained with an imaging spectrometer. The intensity mapping approach measures the spatio-spectral fluctuations due to line emission from all galaxies, including those below the individual detection threshold. The technique provides 3D measurements of galaxy clustering and moments of the galaxy luminosity function. Furthermore, the linear portion of the power spectrum can be used to measure the total line emission intensity including all sources through cosmic time with redshift information naturally encoded. Total line emission, when compared to the total star formation activity and/or other line intensities, reveals evolution of the interstellar conditions of galaxies in aggregate. As a case study, we consider measurement of [CII] autocorrelation in the 0.5 < z < 1.5 epoch, where interloper lines are minimized, using far-IR/submillimeter balloon-borne and future space-borne instruments with moderate and high sensitivity, respectively. In this context, we compare the intensity mapping approach to blind galaxy surveys based on individual detections. We find that intensity mapping is nearly always the best way to obtain the total line emission because blind, wide-field galaxy surveys lack sufficient depth and deep pencil beams do not observe enough galaxies in the requisite luminosity and redshift bins. Also, intensity mapping is often the most efficient way to measure the power spectrum shape, depending on the details of the luminosity function and the telescope aperture.
C1 [Uzgil, B. D.; Aguirre, J. E.; Lidz, A.] Univ Penn, Philadelphia, PA 19104 USA.
   [Uzgil, B. D.; Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Uzgil, BD (reprint author), Univ Penn, Philadelphia, PA 19104 USA.
EM badeu@sas.upenn.edu
FU NASA GSRP Fellowship
FX The authors thank Olivier Dore for useful discussions and Yan Gong for
   valuable comments that improved this manuscript. B.U. acknowledges
   support from the NASA GSRP Fellowship. 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 48
TC 11
Z9 11
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 OCT 1
PY 2014
VL 793
IS 2
AR 116
DI 10.1088/0004-637X/793/2/116
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP3HD
UT WOS:000341965300047
ER

PT J
AU Strangman, GE
   Sipes, W
   Beven, G
AF Strangman, Gary E.
   Sipes, Walter
   Beven, Gary
TI Human Cognitive Performance in Spaceflight and Analogue Environments
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Review
DE long-duration spaceflight; executive function; social processing;
   emotional processing; hippocampus
ID NORMAL-PRESSURE HYDROCEPHALUS; INTERNATIONAL BIOMEDICAL EXPEDITION;
   PROLONGED ANTARCTIC RESIDENCE; MANUAL TRACKING PERFORMANCE; COMPLEX
   DECISION-MAKING; DUAL-TASK PERFORMANCE; CEREBRAL-BLOOD-FLOW; SPACE
   MISSION; MENTAL PERFORMANCE; CARBON-DIOXIDE
AB Maintaining intact cognitive performance is a high priority for space exploration. This review seeks to summarize the cumulative results of existing studies of cognitive performance in spaceflight and analogue environments. We focused on long-duration (>21 d) studies for which no review has previously been conducted. There were 11 published studies identified for long-duration spaceflight (N = 42 subjects) as well as 21 shorter spaceflight studies (N = 70 subjects). Overall, spaceflight cognitive studies ranged from 6-438 d in duration. Some 55 spaceflight analogue studies were also identified, ranging from 6 to 520 d. The diverse nature of experimental procedures and protocols precluded formal meta-analysis. In general, the available evidence fails to strongly support or refute the existence of specific cognitive deficits in low Earth orbit during long-duration spaceflight, which may be due in large part to small numbers of subjects. The studies consistently suggest that novel environments (spaceflight or other) induce variable alterations in cognitive performance across individuals, consistent with known astronaut experiences. This highlights the need to better quantify the magnitude and scope of this interindividual variability, and understand its underlying factors, when predicting in-flight cognitive functioning for extended periods.
C1 [Strangman, Gary E.] Harvard Univ, Sch Med, Dept Psychiat, Boston, MA 02115 USA.
   [Sipes, Walter; Beven, Gary] NASA, Johnson Space Ctr, Houston, TX USA.
RP Strangman, GE (reprint author), Massachusetts Gen Hosp, Neural Syst Grp, 149 13th St,Suite 2651, Charlestown, MA 02129 USA.
EM strang@nmr.mgh.harvard.edu
FU Wyle, Science, Technology and Engineering [T71712]
FX This work was supported by Wyle, Science, Technology and Engineering,
   subcontract number T71712. All authors provided a professional
   contribution to this paper. Special thanks go to Lauren Leveton and
   multiple colleagues in the NASA Human Research Program's Behavioral
   Health and Performance element, as well as to the numerous colleagues
   who provided input on previous versions of this work.
NR 147
TC 5
Z9 5
U1 3
U2 19
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
EI 1943-4448
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD OCT
PY 2014
VL 85
IS 10
BP 1033
EP 1048
DI 10.3357/ASEM.3961.2014
PG 16
WC Public, Environmental & Occupational Health; Medicine, General &
   Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
   Medicine; Sport Sciences
GA AP7MM
UT WOS:000342261400008
PM 25245904
ER

PT J
AU Keeton, KE
   Richard, EE
   Davis, JR
AF Keeton, Kathryn E.
   Richard, Elizabeth E.
   Davis, Jeffrey R.
TI Solution Mechanism Guide: Implementing Innovation Within a Research &
   Development Organization
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Editorial Material
DE open innovation; strategic management; knowledge management; decision
   analysis; decision making; collaboration
AB In order to create a culture more open to novel problem-solving mechanisms, NASA's Human Health and Performance Directorate (HH&P) created a strategic knowledge management tool that educates employees about innovative problem-solving techniques, the Solution Mechanism Guide (SMG). The SMG is a web-based, interactive guide that leverages existing and innovative problem-solving methods and presents this information as a unique user experience so that the employee is empowered to make the best decision about which problem-solving tool best meets their needs. By integrating new and innovative methods with existing problem solving tools, the SMG seamlessly introduces open innovation and collaboration concepts within HH&P to more effectively address human health and performance risks. This commentary reviews the path of creating a more open and innovative culture within HH&P and the process and development steps that were taken to develop the SMG.
C1 [Keeton, Kathryn E.; Richard, Elizabeth E.] Wyle, Houston, TX USA.
   [Davis, Jeffrey R.] NASA, Johnson Space Ctr, Houston, TX USA.
RP Keeton, KE (reprint author), 1290 Hercules, Houston, TX 77058 USA.
EM kathryn.keeton@nasa.gov
NR 9
TC 1
Z9 1
U1 3
U2 12
PU AEROSPACE MEDICAL ASSOC
PI ALEXANDRIA
PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA
SN 0095-6562
EI 1943-4448
J9 AVIAT SPACE ENVIR MD
JI Aviat. Space Environ. Med.
PD OCT
PY 2014
VL 85
IS 10
BP 1061
EP 1062
DI 10.3357/ASEM.4050.2014
PG 2
WC Public, Environmental & Occupational Health; Medicine, General &
   Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
   Medicine; Sport Sciences
GA AP7MM
UT WOS:000342261400013
PM 25245908
ER

PT J
AU Mehta, SK
   Laudenslager, ML
   Stowe, RP
   Crucian, BE
   Sams, CF
   Pierson, DL
AF Mehta, S. K.
   Laudenslager, M. L.
   Stowe, R. P.
   Crucian, B. E.
   Sams, C. F.
   Pierson, D. L.
TI Multiple latent viruses reactivate in astronauts during Space Shuttle
   missions
SO BRAIN BEHAVIOR AND IMMUNITY
LA English
DT Article
DE Epstein-Barr virus; Cytomegalovirus; Varicella-zoster virus; Stress;
   Spaceflight; Cortisol; DHEA
ID EPSTEIN-BARR-VIRUS; IMMUNE-SYSTEM DYSREGULATION; VARICELLA-ZOSTER-VIRUS;
   SALIVARY CORTISOL; BIOLOGICAL MARKER; DURATION MISSIONS; HAIR CORTISOL;
   STRESS; SPACEFLIGHT; DEHYDROEPIANDROSTERONE
AB Latent virus reactivation and diurnal salivary cortisol and dehydroepiandrosterone were measured prospectively in 17 astronauts (16 male and 1 female) before, during, and after short-duration (12-16 days) Space Shuttle missions. Blood, urine, and saliva samples were collected during each of these phases. Antiviral antibodies and viral load (DNA) were measured for Epstein-Barr virus (EBV), varicella-zoster virus (VZV), and cytomegalovirus (CMV). Three astronauts did not shed any virus in any of their samples collected before, during, or after flight. EBV was shed in the saliva in all of the remaining 14 astronauts during all 3 phases of flight. Seven of the 14 EBV-shedding subjects also shed VZV during and after the flight in their saliva samples, and 8 of 14 EBV-shedders also shed CMV in their urine samples before, during, and after flight. In 6 of 14 crewmembers, all 3 target viruses were shed during one or more flight phases. Both EBV and VZV DNA copies were elevated during the flight phase relative to preflight or post-flight levels. EBV DNA in peripheral blood was increased preflight relative to post-flight. Eighteen healthy controls were also included in the study. Approximately 2-5% of controls shed EBV while none shed VZV or CMV. Salivary cortisol measured preflight and during flight were elevated relative to post-flight. In contrast DHEA decreased during the flight phase relative to both preflight and post-flight. As a consequence, the molar ratio of the area under the diurnal curve of cortisol to DHEA with respect to ground (AUCg) increased significantly during flight. This ratio was unrelated to viral shedding. In summary, three herpes viruses can reactivate individually or in combination during spaceflight. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Mehta, S. K.] Enterprise Advisory Serv Inc, Houston, TX 77058 USA.
   [Laudenslager, M. L.] Univ Colorado Denver, Aurora, CO 80045 USA.
   [Stowe, R. P.] Microgen Labs, La Marque, TX 77568 USA.
   [Crucian, B. E.; Sams, C. F.; Pierson, D. L.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
RP Mehta, SK (reprint author), Enterprise Advisory Serv Inc, 1290 Hercules, Houston, TX 77058 USA.
EM satish.k.mehta@nasa.gov; Mark.Laudenslager@ucdenver.edu;
   rpstowe@microgenlabs.com; brian.crucian-1@nasa.gov;
   clarence.sams-1@nasa.gov; duane.l.pierson@nasa.gov
OI Laudenslager, Mark/0000-0002-9815-3026
FU NASA [111-30-10-03, 111-30-10-06]
FX We gratefully acknowledge the participation of the astronauts in the
   study. We appreciate the expert processing of the saliva samples by Mark
   Goldstein and Patrick Benitez, and the assistance of Crystal Natvig in
   data processing and figure preparation. We thank Jane Krauhs for
   editorial assistance. We also thank Alan Feiveson for statistical
   analysis. We thank the astute reviewers for early suggestions that led
   to a reanalysis of the diurnal steroid data. This work was supported by
   NASA grants 111-30-10-03 and 111-30-10-06 to DLP.
NR 45
TC 12
Z9 12
U1 5
U2 15
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0889-1591
EI 1090-2139
J9 BRAIN BEHAV IMMUN
JI Brain Behav. Immun.
PD OCT
PY 2014
VL 41
BP 210
EP 217
DI 10.1016/j.bbi.2014.05.014
PG 8
WC Immunology; Neurosciences
SC Immunology; Neurosciences & Neurology
GA AP2MD
UT WOS:000341905400024
PM 24886968
ER

PT J
AU Dresing, N
   Cohen, CMS
   Gomez-Herrero, R
   Heber, B
   Klassen, A
   Leske, RA
   Mason, GM
   Mewaldt, RA
   von Rosenvinge, TT
AF Dresing, N.
   Cohen, C. M. S.
   Gomez-Herrero, R.
   Heber, B.
   Klassen, A.
   Leske, R. A.
   Mason, G. M.
   Mewaldt, R. A.
   von Rosenvinge, T. T.
TI Approaching Solar Maximum 24 with STEREO-Multipoint Observations of
   Solar Energetic Particle Events
SO BRAZILIAN JOURNAL OF PHYSICS
LA English
DT Article; Proceedings Paper
CT 33rd International Cosmic Ray Conference (ICRC)
CY 2013
CL Rio de Janeiro, BRAZIL
DE Solar energetic particle (SEP) events
ID SPACECRAFT OBSERVATIONS; INNER HELIOSPHERE; PEAK INTENSITIES;
   ACCELERATION; TRANSPORT; DEPENDENCE; SECCHI; SUN
AB Since the beginning of the Solar Terrestrial Relations Observatory (STEREO) mission at the end of 2006, the two spacecraft have now separated by more than 130 (a similar to) degrees from the Earth. A 360-degree view of the Sun has been possible since February 2011, providing multipoint in situ and remote sensing observations of unprecedented quality. Combining STEREO observations with near-Earth measurements allows the study of solar energetic particle (SEP) events over a wide longitudinal range with minimal radial gradient effects. This contribution provides an overview of recent results obtained by the STEREO/IMPACT team in combination with observations by the ACE and SOHO spacecraft. We focus especially on multi-spacecraft investigations of SEP events. The large longitudinal spread of electron and He-3-rich events as well as unusual anisotropies will be presented and discussed.
C1 [Dresing, N.; Heber, B.; Klassen, A.] Univ Kiel, IEAP, Kiel, Germany.
   [Cohen, C. M. S.; Leske, R. A.; Mewaldt, R. A.] CALTECH, Pasadena, CA 91125 USA.
   [Gomez-Herrero, R.] Univ Alcala De Henares, Space Res Grp, Alcala De Henares, Spain.
   [Mason, G. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
   [von Rosenvinge, T. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Dresing, N (reprint author), Univ Kiel, IEAP, Kiel, Germany.
EM dresing@physik.uni-kiel.de
RI Gomez-Herrero, Raul/B-7346-2011
OI Gomez-Herrero, Raul/0000-0002-5705-9236
NR 42
TC 1
Z9 1
U1 0
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0103-9733
EI 1678-4448
J9 BRAZ J PHYS
JI Braz. J. Phys.
PD OCT
PY 2014
VL 44
IS 5
BP 504
EP 511
DI 10.1007/s13538-014-0227-5
PG 8
WC Physics, Multidisciplinary
SC Physics
GA AP6CL
UT WOS:000342165000008
ER

PT J
AU Jones, WV
AF Jones, William Vernon
TI Highlights of the NASA Particle Astrophysics Program
SO BRAZILIAN JOURNAL OF PHYSICS
LA English
DT Article
DE Cosmic rays; Particle astrophysics; Balloons; LDB; ULDB; ISS observatory
AB The NASA Particle Astrophysics Program covers Origin of the Elements, Nearest Sources of Cosmic Rays, How Cosmic Particle Accelerators Work, The Nature of Dark Matter, and Neutrino Astrophysics. Progress in each of these topics has come from sophisticated instrumentation flown on long duration balloon (LDB) flights around Antarctica over the past two decades. New opportunities including Super Pressure Balloons (SPB) and International Space Station (ISS) platforms are emerging for the next major step. Stable altitudes and long durations enabled by SPB flights ensure ultra-long duration balloon (ULDB) missions that can open doors to new science opportunities. The Alpha Magnetic Spectrometer (AMS) has been operating on the ISS since May 2011. The CALorimetric Electron Telescope (CALET) and Cosmic Ray Energetics And Mass (CREAM) experiments are being developed for launch to the Japanese Experiment Module Exposed Facility (JEM-EF) in 2014. And, the Extreme Universe Space Observatory (EUSO) is planned for launch to the ISS JEM-EF after 2017. Collectively, these four complementary ISS missions covering a large portion of the cosmic ray energy spectrum serve as a cosmic ray observatory.
C1 NASA Headquarters, Astrophys Div DH000, Sci Mission Directorate, Washington, DC 20546 USA.
RP Jones, WV (reprint author), NASA Headquarters, Astrophys Div DH000, Sci Mission Directorate, Washington, DC 20546 USA.
EM w.vernon.jones@nasa.gov
NR 12
TC 1
Z9 1
U1 1
U2 10
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0103-9733
EI 1678-4448
J9 BRAZ J PHYS
JI Braz. J. Phys.
PD OCT
PY 2014
VL 44
IS 5
BP 534
EP 539
DI 10.1007/s13538-014-0247-1
PG 6
WC Physics, Multidisciplinary
SC Physics
GA AP6CL
UT WOS:000342165000012
ER

PT J
AU Parazoo, NC
   Bowman, K
   Fisher, JB
   Frankenberg, C
   Jones, DBA
   Cescatti, A
   Perez-Priego, O
   Wohlfahrt, G
   Montagnani, L
AF Parazoo, Nicholas C.
   Bowman, Kevin
   Fisher, Joshua B.
   Frankenberg, Christian
   Jones, Dylan B. A.
   Cescatti, Alessandro
   Perez-Priego, Oscar
   Wohlfahrt, Georg
   Montagnani, Leonardo
TI Terrestrial gross primary production inferred from satellite
   fluorescence and vegetation models
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE amazon; carbon cycle; climate change; flux towers; model benchmarking;
   water stress
ID NET ECOSYSTEM EXCHANGE; SUN-INDUCED FLUORESCENCE; CARBON-CYCLE MODELS;
   CHLOROPHYLL FLUORESCENCE; PLANT GEOGRAPHY; CLIMATE-CHANGE; CO2;
   DYNAMICS; ASSIMILATION; SPACE
AB Determining the spatial and temporal distribution of terrestrial gross primary production (GPP) is a critical step in closing the Earth's carbon budget. Dynamical global vegetation models (DGVMs) provide mechanistic insight into GPP variability but diverge in predicting the response to climate in poorly investigated regions. Recent advances in the remote sensing of solar-induced chlorophyll fluorescence (SIF) opens up a new possibility to provide direct global observational constraints for GPP. Here, we apply an optimal estimation approach to infer the global distribution of GPP from an ensemble of eight DGVMs constrained by global measurements of SIF from the Greenhouse Gases Observing SATellite (GOSAT). These estimates are compared to flux tower data in N. America, Europe, and tropical S. America, with careful consideration of scale differences between models, GOSAT, and flux towers. Assimilation of GOSAT SIF with DGVMs causes a redistribution of global productivity from northern latitudes to the tropics of 7-8PgCyr(-1) from 2010 to 2012, with reduced GPP in northern forests (similar to 3.6PgCyr(-1)) and enhanced GPP in tropical forests (similar to 3.7PgCyr(-1)). This leads to improvements in the structure of the seasonal cycle, including earlier dry season GPP loss and enhanced peak-to-trough GPP in tropical forests within the Amazon Basin and reduced growing season length in northern croplands and deciduous forests. Uncertainty in predicted GPP (estimated from the spread of DGVMs) is reduced by 40-70% during peak productivity suggesting the assimilation of GOSAT SIF with models is well-suited for benchmarking. We conclude that satellite fluorescence augurs a new opportunity to quantify the GPP response to climate drivers and the potential to constrain predictions of carbon cycle evolution.
C1 [Parazoo, Nicholas C.; Bowman, Kevin; Fisher, Joshua B.; Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Parazoo, Nicholas C.; Bowman, Kevin; Jones, Dylan B. A.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
   [Jones, Dylan B. A.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
   [Cescatti, Alessandro] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy.
   [Perez-Priego, Oscar] Univ Granada, Dept Fis Aplicada, E-18071 Granada, Spain.
   [Wohlfahrt, Georg] Univ Innsbruck, Inst Okol, A-6020 Innsbruck, Austria.
   [Montagnani, Leonardo] Autonomous Prov Bolzano, Forest Serv, I-39100 Bolzano, Italy.
   [Montagnani, Leonardo] Free Univ Bolzano, Fac Sci & Technol, I-39100 Bolzano, Italy.
RP Parazoo, NC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM nicholas.c.parazoo@jpl.nasa.gov
RI Jones, Dylan/O-2475-2014; Wohlfahrt, Georg/D-2409-2009; Montagnani,
   Leonardo/F-1837-2016; Frankenberg, Christian/A-2944-2013; 
OI Jones, Dylan/0000-0002-1935-3725; Wohlfahrt, Georg/0000-0003-3080-6702;
   Montagnani, Leonardo/0000-0003-2957-9071; Frankenberg,
   Christian/0000-0002-0546-5857; Fisher, Joshua/0000-0003-4734-9085
FU U.S. Department of Energy, Biological and Environmental Research,
   Terrestrial Carbon Program [DE-FG02-04ER63917, DE-FG02-04ER63911];
   CFCAS; NSERC; BIOCAP; Environment Canada; NRCan; CarboEuropeIP;
   FAO-GTOS-TCO; iLEAPS; Max Planck Institute for Biogeochemistry; National
   Science Foundation; University of Tuscia; Universite Laval and
   Environment Canada; US Department of Energy; NSF [0845166];
   Fluxnet-Canada Research Network (FCRN) [2002-07]; Canadian Carbon
   Program (CCP) [2007-11]; Canadian Foundation for Climate and Atmospheric
   Sciences (CFCAS); Canadian Natural Sciences and Engineering Research
   Council (NSERC); Canadian Forest Service (CFS); Ontario Ministry of
   Environment; NASA [NNX10AT42G]; NASA;  [FAPESP-0858120-3]
FX We thank M. Reichstein for providing the MPI-BGC dataset. We acknowledge
   all MODIS land product science team members for providing an invaluable
   public dataset. The improved MOD17 GPP data were provided by the
   Numerical Terradynamic Simulation Group at the University of Montana. We
   thank the Global Carbon Project and TRENDY modelers for contributing
   model output: S. Sitch and C. Huntingford (TRIF-FID/JULES), B. Poulter
   (LPJ), A. Ahlstrom (LPJ-GUESS), M. Lomas (SDGVM), S. Levis (CLM4CN), S.
   Zaehle (OCN), N. Viovy (Orchidee), and N. Zeng (VEGAS). We also give
   special thanks to S Sitch and P Friedlingstein for organizing TRENDY and
   for valuable discussions regarding this work. This work used eddy
   covariance data acquired by the FLUXNET community and in particular by
   the following networks: AmeriFlux (U.S. Department of Energy, Biological
   and Environmental Research, Terrestrial Carbon Program
   (DE-FG02-04ER63917 and DE-FG02-04ER63911)), CarboEuropeIP, CarboItaly,
   CarboMont, Fluxnet-Canada (supported by CFCAS, NSERC, BIOCAP,
   Environment Canada, and NRCan), GreenGrass, KoFlux, LBA (Partial funding
   provided by FAPESP-0858120-3), NECC, USCCC. We acknowledge the financial
   support to the eddy covariance data harmonization provided by
   CarboEuropeIP, FAO-GTOS-TCO, iLEAPS, Max Planck Institute for
   Biogeochemistry, National Science Foundation, University of Tuscia,
   Universite Laval and Environment Canada, and US Department of Energy and
   the database development and technical support from Berkeley Water
   Center, Lawrence Berkeley National Laboratory, Microsoft Research
   eScience, Oak Ridge National Laboratory, University of California -
   Berkeley, University of Virginia. Funding for US-PFa is provided by NSF
   Award #0845166. We acknowledge the receipt of data from the Groundhog
   River site (CA-OMW) collected under the auspices of the Fluxnet-Canada
   Research Network (FCRN, 2002-07) and the Canadian Carbon Program (CCP,
   2007-11) with funding support from the Canadian Foundation for Climate
   and Atmospheric Sciences (CFCAS), the Canadian Natural Sciences and
   Engineering Research Council (NSERC), the Canadian Forest Service (CFS),
   and the Ontario Ministry of Environment. We give special thanks to H.
   McCaughey (CA-OMW), R. Huc (FR-FBN), N. Buchmann (CH-Lae, CH-Oe2,
   CH-Dav), N. Restrepo-Coupe (LBA), G. Bohrer (US-UMd), A. Desai (US-PFa)
   for contributing flux tower data and providing valuable discussions.
   This research was funded by the NASA Atmospheric CO<INF>2</INF>
   Observations from Space (ACOS) program (grant number NNX10AT42G), and
   carried out at the Jet Propulsion Laboratory, California Institute of
   Technology, under a contract with NASA (c) 2013.
NR 58
TC 24
Z9 25
U1 13
U2 120
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
EI 1365-2486
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD OCT
PY 2014
VL 20
IS 10
BP 3103
EP 3121
DI 10.1111/gcb.12652
PG 19
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA AP6DU
UT WOS:000342168500010
PM 24909755
ER

PT J
AU Melachroinos, SA
   Lemoine, FG
   Chinn, DS
   Zelensky, NP
   Nicholas, JB
   Beckley, BD
AF Melachroinos, Stavros A.
   Lemoine, Frank G.
   Chinn, Douglas S.
   Zelensky, Nikita P.
   Nicholas, Joseph B.
   Beckley, Brian D.
TI The effect of seasonal and long-period geopotential variations on the
   GPS orbits
SO GPS SOLUTIONS
LA English
DT Article
DE GPS; Time-varying gravity; Reference frame; Orbit determination
ID TIME-SERIES; POSITION; GRAVITY
AB We examine the impact of using seasonal and long-period time-variable gravity field (TVG) models on GPS orbit determination, through simulations from 1994 to 2012. The models of time-variable gravity that we test include the GRGS release RL02 GRACE-derived 10-day gravity field models up to degree and order 20 (grgs20x20), a 4 x 4 series of weekly coefficients using GGM03S as a base derived from SLR and DORIS tracking to 11 satellites (tvg4x4), and a harmonic fit to the above 4 x 4 SLR-DORIS time series (goco2s_fit2). These detailed models are compared to GPS orbit simulations using a reference model (stdtvg) based on the International Earth Rotation Service (IERS) and International GNSS Service (IGS) repro1 standards. We find that the new TVG modeling produces significant along, cross-track orbit differences as well as annual, semi-annual, draconitic and long-period effects in the Helmert translation parameters (Tx, Ty, Tz) of the GPS orbits with magnitudes of several mm. We show that the simplistic TVG modeling approach used by all of the IGS Analysis Centers, which is based on the models provided by the IERS standards, becomes progressively less adequate following 2006 when compared to the seasonal and long-period TVG models.
C1 [Melachroinos, Stavros A.; Chinn, Douglas S.; Zelensky, Nikita P.; Beckley, Brian D.] SGT Inc, Div Sci, Greenbelt, MD 20770 USA.
   [Melachroinos, Stavros A.; Lemoine, Frank G.; Chinn, Douglas S.; Zelensky, Nikita P.; Nicholas, Joseph B.; Beckley, Brian D.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
   [Nicholas, Joseph B.] Emergent Space Technol, Greenbelt, MD 20770 USA.
RP Melachroinos, SA (reprint author), SGT Inc, Div Sci, 7701 Greenbelt Rd, Greenbelt, MD 20770 USA.
EM Smelachroinos@sgt-inc.com; Frank.g.lemoine@nasa.gov;
   Douglas.s.chinn@nasa.gov; Nzelensky@sgt-inc.com;
   Nicholas@emergentspace.com; Brian.D.Beckley@nasa.gov
RI Lemoine, Frank/D-1215-2013
FU US National Aeronautics and Space Administration (NASA)
FX We acknowledge the International GNSS Service (IGS) for its support and
   leadership in providing precise GPS orbits as well as Jim Ray, one
   anonymous reviewer and Prof. Alfred Leick for their suggestions and
   remarks. J.-P. Boy (University of Strasbourg, France) provided the
   atmospheric gravity time series derived from ECMWF pressure fields. This
   research was supported by the US National Aeronautics and Space
   Administration (NASA) under the program "IDS Program in Mean Sea Level."
NR 41
TC 2
Z9 2
U1 2
U2 14
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1080-5370
EI 1521-1886
J9 GPS SOLUT
JI GPS Solut.
PD OCT
PY 2014
VL 18
IS 4
BP 497
EP 507
DI 10.1007/s10291-013-0346-4
PG 11
WC Remote Sensing
SC Remote Sensing
GA AP5XE
UT WOS:000342151200002
ER

PT J
AU Crucian, BE
   Zwart, SR
   Mehta, S
   Uchakin, P
   Quiriarte, HD
   Pierson, D
   Sams, CF
   Smith, SM
AF Crucian, Brian E.
   Zwart, Sara R.
   Mehta, Satish
   Uchakin, Peter
   Quiriarte, Heather D.
   Pierson, Duane
   Sams, Clarence F.
   Smith, Scott M.
TI Plasma Cytokine Concentrations Indicate That In Vivo Hormonal Regulation
   of Immunity Is Altered During Long-Duration Spaceflight
SO JOURNAL OF INTERFERON AND CYTOKINE RESEARCH
LA English
DT Article
ID MACROPHAGE INFLAMMATORY PROTEIN-1; HINDLIMB-UNLOADING MODEL;
   EPSTEIN-BARR-VIRUS; T-CELL-ACTIVATION; SPACE-FLIGHT; SYSTEM
   DYSREGULATION; PLATELET CHEMOKINES; DISEASE; MICROGRAVITY; ASTRONAUTS
AB Aspects of immune system dysregulation associated with long-duration spaceflight have yet to be fully characterized and may represent a clinical risk to crewmembers during deep space missions. Plasma cytokine concentration may serve as an indicator of in vivo physiological changes or immune system mobilization. The plasma concentrations of 22 cytokines were monitored in 28 astronauts during long-duration spaceflight onboard the International Space Station. Blood samples were collected 3 times before flight, 3-5 times during flight (depending on mission duration), at landing, and 30 days after landing. Analysis was performed by bead array immunoassay. With few exceptions, minimal detectable mean plasma concentrations were observed at baseline (launch minus 180) for innate inflammatory cytokines or adaptive regulatory cytokines; however, interleukin (IL)-1ra and several chemokines and growth factors were constitutively present. An increase in the plasma concentration, tumor necrosis factor-alpha (TNF alpha), IL-8, IL-1ra, thrombopoietin (Tpo), vascular endothelial growth factor (VEGF), C-C motif chemokine ligand 2 (CCL2), chemokine ligand 4/macrophage inhibitory protein 1b (CCL4), and C-X-C motif chemokine 5/epithelial neutrophil-activating protein 78 (CXCL5) was observed associated with spaceflight. No significant alterations were observed during or following spaceflight for the inflammatory or adaptive/T-regulatory cytokines: IL-1 alpha, IL-1 beta, IL-2, interferon-gamma (IFN-gamma), IL-17, IL-4, IL-5, IL-10, G-CSF, GM-CSF, FGF basic, CCL3, or CCL5. This pattern of cytokine dysregulation suggests multiple physiological adaptations persist during flight, including inflammation, leukocyte recruitment, angiogenesis, and thrombocyte regulation.
C1 [Crucian, Brian E.; Pierson, Duane; Sams, Clarence F.; Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
   [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX USA.
   [Mehta, Satish] EASI, Houston, TX USA.
   [Uchakin, Peter] Mercer Univ, Macon, GA 31207 USA.
   [Quiriarte, Heather D.] JES Tech, Houston, TX USA.
RP Crucian, BE (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mail Code SK4, Houston, TX 77058 USA.
EM brian.crucian-1@nasa.gov
NR 49
TC 12
Z9 12
U1 1
U2 8
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1079-9907
EI 1557-7465
J9 J INTERF CYTOK RES
JI J. Interferon Cytokine Res.
PD OCT 1
PY 2014
VL 34
IS 10
BP 778
EP 786
DI 10.1089/jir.2013.0129
PG 9
WC Biochemistry & Molecular Biology; Cell Biology; Immunology
SC Biochemistry & Molecular Biology; Cell Biology; Immunology
GA AQ1SR
UT WOS:000342561800005
PM 24702175
ER

PT J
AU Wei, M
   Zhang, J
   Fryauf, DM
   Leon, JJD
   Norris, KJ
   Deng, H
   Wen, GJ
   Wang, SY
   Kobayashi, NP
AF Wei, Min
   Zhang, Junce
   Fryauf, David M.
   Leon, Juan J. Diaz
   Norris, Kate J.
   Deng, Hong
   Wen, Guangjun
   Wang, Shih-Yuan
   Kobayashi, Nobuhiko P.
TI Growth and characterization of indium phosphide nanowires on transparent
   conductive ZnO:Al films
SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS
LA English
DT Article
ID DEPENDENT PHOTOLUMINESCENCE; INP NANOWIRES
AB The epitaxial growth of indium phosphide nanowires (InP NWs) on transparent conductive aluminum-doped zinc oxide (ZnO:Al) thin films is proposed and demonstrated. ZnO:Al thin films were prepared on quartz substrates by radio frequency magnetron sputtering, then InP NWs were grown on them by plasma enhanced metal organic chemical vapor deposition with gold catalyst. Microstructure and optical properties of InP nanowires on ZnO:Al thin films were investigated by X-ray diffraction (XRD), scanning electron microscopy (SEM), X-ray photoelectric spectroscopy (XPS), photoluminescence and Raman spectroscopy at room temperature. SEM shows that randomly oriented and intersecting InP nanowires were grown to form a network on ZnO:Al thin films. Both wurtzite (WZ) and zincblende (ZB) structures coexist in the random orientation InP NWs on ZnO:Al thin film had been proved by XRD analysis. XPS result indicates Zn diffusion exists in the InP NWs on ZnO:Al. The photoluminescence spectra of InP nanowires with Zn diffusion present an emission at 915 nm. Zn diffusion also bring effect on Raman spectra of InP NWs, leading to more Raman-shift and larger relative intensity ratio of TO/LO.
C1 [Wei, Min; Deng, Hong] Univ Elect Sci & Technol China, Sch Microelect & Solid Elect, Chengdu 610054, Peoples R China.
   [Wei, Min; Zhang, Junce; Fryauf, David M.; Leon, Juan J. Diaz; Norris, Kate J.; Wang, Shih-Yuan; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.
   [Zhang, Junce; Fryauf, David M.; Leon, Juan J. Diaz; Norris, Kate J.; Wang, Shih-Yuan; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, NASA Ames Res Ctr, Nanostruct Energy Convers Technol & Res NECTAR, Adv Studies Labs, Moffett Field, CA 94035 USA.
   [Wen, Guangjun] Univ Elect Sci & Technol China, Sch Commun & Informat Engn, Chengdu 610054, Peoples R China.
RP Wei, M (reprint author), Univ Elect Sci & Technol China, Sch Microelect & Solid Elect, Chengdu 610054, Peoples R China.
EM minwei@uestc.edu.cn
RI Kobayashi, Nobuhiko/E-3834-2012
FU National Science Foundation [DGE-0809125-006]; Fundamental Research
   Funds for the Central Universities of China [ZYGX2013J041]; Innovation
   Fund project of the State Key Laboratory of Electronic Thin Films and
   Integrated Devices of China [KFJJ201303]; Research Fund for the Doctoral
   Program of Higher Education of China [20110185110014]
FX This work was supported by the National Science Foundation Graduate
   Research Fellowship under Grant No. DGE-0809125-006, and it also was
   supported by Fundamental Research Funds for the Central Universities of
   China (ZYGX2013J041), Innovation Fund project of the State Key
   Laboratory of Electronic Thin Films and Integrated Devices of China
   (KFJJ201303), and Research Fund for the Doctoral Program of Higher
   Education of China (20110185110014).
NR 20
TC 3
Z9 3
U1 0
U2 32
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0957-4522
EI 1573-482X
J9 J MATER SCI-MATER EL
JI J. Mater. Sci.-Mater. Electron.
PD OCT
PY 2014
VL 25
IS 10
BP 4444
EP 4449
DI 10.1007/s10854-014-2186-6
PG 6
WC Engineering, Electrical & Electronic; Materials Science,
   Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA AP5ZP
UT WOS:000342157500038
ER

PT J
AU Zambrano, HA
   Walther, JH
   Jaffe, RL
AF Zambrano, H. A.
   Walther, J. H.
   Jaffe, R. L.
TI Molecular dynamics simulations of water on a hydrophilic silica surface
   at high air pressures
SO JOURNAL OF MOLECULAR LIQUIDS
LA English
DT Article
DE Molecular dynamics; Wetting; Nanodroplets; Contact angle;
   Solid-liquid-gas interactions
ID ATOMIC-FORCE MICROSCOPY; CARBON NANOTUBES; HYDROPHOBIC SURFACES;
   CONTACT-ANGLE; NANOFLUIDIC CHANNELS; AQUEOUS-SOLUTIONS; AMORPHOUS
   SILICA; SOLID-SURFACE; FLOW; NANOCHANNELS
AB We present a force field for Molecular Dynamics (MD) simulations of water and air in contact with an amorphous silica surface. We calibrate the interactions of each species present in the system using dedicated criteria such as the contact angle of a water droplet on a silica surface, and the solubility of air in water at different pressures. Using the calibrated force field, we conduct MD simulations to study the interface between a hydrophilic silica substrate and water surrounded by air at different pressures. We find that the static water contact angle is independent of the air pressure imposed on the system. Our simulations reveal the presence of a nanometer thick layer of gas at the water-silica interface. We believe that this gas layer could promote nucleation and stabilization of surface nanobubbles at amorphous silica surfaces. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Zambrano, H. A.] Univ Concepcion, Dept Chem Engn, Concepcion, Chile.
   [Walther, J. H.] Tech Univ Denmark, Dept Mech Engn, DK-2800 Lyngby, Denmark.
   [Walther, J. H.] ETH, Chair Computat Sci, CH-8092 Zurich, Switzerland.
   [Jaffe, R. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Walther, JH (reprint author), Tech Univ Denmark, Dept Mech Engn, DK-2800 Lyngby, Denmark.
EM jhw@mek.dtu.dk
RI Walther, Jens/D-9549-2015; 
OI Walther, Jens/0000-0001-8100-9178; Zambrano, Harvey/0000-0003-1049-8482
FU Danish Research Council [274-06-0465]; Myhrwold Foundation; Otto Monsted
   Foundation
FX Support for this work is provided in part by the Danish Research Council
   (grant no. 274-06-0465), and the Myhrwold, and Otto Monsted Foundations.
   The authors wish to acknowledge discussion with Petros Koumoutsakos and
   computational support from the Danish Center for Scientific Computing
   (DCSC).
NR 96
TC 6
Z9 6
U1 3
U2 44
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-7322
EI 1873-3166
J9 J MOL LIQ
JI J. Mol. Liq.
PD OCT
PY 2014
VL 198
BP 107
EP 113
DI 10.1016/j.molliq.2014.06.003
PG 7
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA AP7GG
UT WOS:000342245200015
ER

PT J
AU Butner, JE
   Dyer, HL
   Malloy, TS
   Kranz, LV
AF Butner, Jonathan E.
   Dyer, H. Lawrence
   Malloy, Thomas S.
   Kranz, Lucy V.
TI Uncertainty in Cost Performance as a Function of the Cusp Catastrophe in
   the NASA Program Performance Management System
SO NONLINEAR DYNAMICS PSYCHOLOGY AND LIFE SCIENCES
LA English
DT Article
DE cusp catastrophe; multilevel model; performance management system; cost
   performance; uncertainty
ID MULTIMODAL DISTRIBUTIONS; MODEL; TURNOVER
AB Cost performance by NASA programs can generate two stable states within the organization system used for program performance management. These states could be stable individually or show multistability with cusp-like behavior. To test this, we constructed a cusp catastrophe model in a multilevel modeling (HLM) procedure on the cost components of an eleven-month period of one NASA program. HLM was used for its ability to estimate random effects as replacements for unknown control parameters. The cusp catastrophe model was a good description of the data and there was some evidence that the overall budget size functioned as a control parameter. Results are presented in terms of three different forms of uncertainty: attractor strength, unistability or multistability, and control parameters. Recommendations and future directions are focused towards understanding the cause of uncertainty in complex management systems.
C1 [Butner, Jonathan E.; Malloy, Thomas S.] Univ Utah, Salt Lake City, UT 84112 USA.
   [Dyer, H. Lawrence; Kranz, Lucy V.] NASA, Houston, TX USA.
RP Butner, JE (reprint author), Univ Utah, Dept Psychol, 380 S 1530 E,Room 502, Salt Lake City, UT 84112 USA.
EM jonathan.butner@psych.utah.edu
NR 38
TC 1
Z9 1
U1 0
U2 5
PU SOC CHAOS THEORY PSYCHOLOGY & LIFE SCIENCES
PI PEWAUKEE
PA W282 N4302 SOMERSET LN, PEWAUKEE, WI 53072 USA
SN 1090-0578
EI 1573-6652
J9 NONLIN DYNAM PSYCHOL
JI Nonlinear Dyn. Psychol. Life Sci.
PD OCT
PY 2014
VL 18
IS 4
BP 397
EP 417
PG 21
WC Social Sciences, Mathematical Methods; Psychology, Mathematical
SC Mathematical Methods In Social Sciences; Psychology
GA AP4LL
UT WOS:000342048200003
PM 25196707
ER

PT J
AU Krucker, S
   Christe, S
   Glesener, L
   Ishikawa, SN
   Ramsey, B
   Takahashi, T
   Watanabe, S
   Saito, S
   Gubarev, M
   Kilaru, K
   Tajima, H
   Tanaka, T
   Turin, P
   McBride, S
   Glaser, D
   Fermin, J
   White, S
   Lin, R
AF Krucker, Saem
   Christe, Steven
   Glesener, Lindsay
   Ishikawa, Shin-Nosuke
   Ramsey, Brian
   Takahashi, Tadayuki
   Watanabe, Shin
   Saito, Shinya
   Gubarev, Mikhail
   Kilaru, Kiranmayee
   Tajima, Hiroyasu
   Tanaka, Takaaki
   Turin, Paul
   McBride, Stephen
   Glaser, David
   Fermin, Jose
   White, Stephen
   Lin, Robert
TI FIRST IMAGES FROM THE FOCUSING OPTICS X-RAY SOLAR IMAGER
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE instrumentation: miscellaneous; Sun: corona; Sun: flares; Sun: X-rays,
   gamma rays
ID RHESSI OBSERVATIONS; QUIET SUN; TELESCOPE; FLARES
AB The Focusing Optics X-ray Solar Imager (FOXSI) sounding rocket payload flew for the first time on 2012 November 2, producing the first focused images of the Sun above 5 keV. To enable hard X-ray (HXR) imaging spectroscopy via direct focusing, FOXSI makes use of grazing-incidence replicated optics combined with fine-pitch solid-state detectors. On its first flight, FOXSI observed several targets that included active regions, the quiet Sun, and a GOES-class B2.7 microflare. This Letter provides an introduction to the FOXSI instrument and presents its first solar image. These data demonstrate the superiority in sensitivity and dynamic range that is achievable with a direct HXR imager with respect to previous, indirect imaging methods, and illustrate the technological readiness for a spaceborne mission to observe HXRs from solar flares via direct focusing optics.
C1 [Krucker, Saem; Glesener, Lindsay; Turin, Paul; McBride, Stephen; Glaser, David; Fermin, Jose; Lin, Robert] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Krucker, Saem] Univ Appl Sci & Arts Northwestern Switzerland, Windisch, Switzerland.
   [Christe, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Ishikawa, Shin-Nosuke] Natl Astron Observ, Mitaka, Tokyo 181, Japan.
   [Ramsey, Brian; Gubarev, Mikhail; Kilaru, Kiranmayee] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
   [Takahashi, Tadayuki; Watanabe, Shin; Saito, Shinya] Inst Space & Astronaut Sci ISAS JAXA, Sagamihara, Kanagawa, Japan.
   [Takahashi, Tadayuki; Watanabe, Shin; Saito, Shinya] Univ Tokyo, Dept Phys, Tokyo 113, Japan.
   [Tajima, Hiroyasu] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
   [Tanaka, Takaaki] Kyoto Univ, Dept Phys, Kyoto 606, Japan.
   [White, Stephen] Air Force Res Lab, Albuquerque, NM USA.
RP Krucker, S (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
OI Glesener, Lindsay/0000-0001-7092-2703; Christe,
   Steven/0000-0001-6127-795X
FU NASA LCAS grant [NNX08AH42G]; NASA GSRP fellowship [NNX09AM40H]; NASA
   contract [NAS 5-98033]
FX FOXSI was funded by NASA LCAS grant NNX08AH42G and received support from
   NASA GSRP fellowship NNX09AM40H. RHESSI work is supported by NASA
   contract NAS 5-98033. The team is grateful to JAXA/ISAS for the donation
   of detectors and ASICs. We thank the members of the NSROC teams at WSMR
   and Wallops for the excellent operation of their systems. We also thank
   the numerous members of the RHESSI and SSL communities who contributed
   advice and help to the project, particularly Hugh Hudson and Gordon
   Hurford for providing helpful advice on this Letter.
NR 25
TC 16
Z9 16
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 1
PY 2014
VL 793
IS 2
AR L32
DI 10.1088/2041-8205/793/2/L32
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP2ES
UT WOS:000341885900011
ER

PT J
AU Macek, WM
   Wawrzaszek, A
   Burlaga, LF
AF Macek, W. M.
   Wawrzaszek, A.
   Burlaga, L. F.
TI MULTIFRACTAL STRUCTURES DETECTED BY VOYAGER 1 AT THE HELIOSPHERIC
   BOUNDARIES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: magnetic fields; solar wind; Sun: heliosphere; turbulence
ID FIELD STRENGTH FLUCTUATIONS; FULLY-DEVELOPED TURBULENCE; MAGNETIC-FIELD;
   INTERSTELLAR PLASMA; SINGULARITY SPECTRUM; HELIOPAUSE; HELIOSHEATH; AU;
   TRANSPORT; MODEL
AB To better understand the dynamics of turbulent systems, we have proposed a phenomenological model based on a generalized Cantor set with two rescaling and one weight parameters. In this Letter, using recent Voyager 1 magnetic field data, we extend our two-scale multifractal analysis further in the heliosheath beyond the heliospheric termination shock, and even now near the heliopause, when entering the interstellar medium for the first time in human history. We have identified the scaling inertial region for magnetized heliospheric plasma between the termination shock and the heliopause. We also show that the degree of multifractality decreases with the heliocentric distance and is still modulated by the phases of the solar cycle in the entire heliosphere including the heliosheath. Moreover, we observe the change of scaling toward a nonintermittent (nonmultifractal) behavior in the nearby interstellar medium, just beyond the heliopause. We argue that this loss of multifractal behavior could be a signature of the expected crossing of the heliopause by Voyager 2 in the near future. The results obtained demonstrate that our phenomenological multifractal model exhibits some properties of intermittent turbulence in the solar system plasmas, and we hope that it could shed light on universal characteristics of turbulence.
C1 [Macek, W. M.] Cardinal Stefan Wyszynski Univ, Fac Math & Nat Sci, PL-01938 Warsaw, Poland.
   [Macek, W. M.; Wawrzaszek, A.] Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland.
   [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Macek, WM (reprint author), Cardinal Stefan Wyszynski Univ, Fac Math & Nat Sci, Woycickiego 1-3, PL-01938 Warsaw, Poland.
EM macek@cbk.waw.pl; anna.wawrzaszek@cbk.waw.pl; lburlagahsp@verizon.net
FU European Community [313038/STORM]; NASA [NNG14PN24P]
FX W.M.M. acknowledges participation in ISSI International Team 318. This
   work was supported by the European Community's Seventh Framework
   Programme ([FP7/2007-2013]) under grant agreement No. 313038/STORM, and
   L.F.B. was supported by NASA NNG14PN24P.
NR 35
TC 4
Z9 4
U1 1
U2 13
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 OCT 1
PY 2014
VL 793
IS 2
AR L30
DI 10.1088/2041-8205/793/2/L30
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP2ES
UT WOS:000341885900009
ER

PT J
AU Schwartz, RA
   Torre, G
   Piana, M
AF Schwartz, R. A.
   Torre, G.
   Piana, M.
TI SYSTEMATIC DE-SATURATION OF IMAGES FROM THE ATMOSPHERIC IMAGING ASSEMBLY
   IN THE SOLAR DYNAMICS OBSERVATORY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: flares; Sun: UV radiation; techniques: image processing
ID LIKELIHOOD; RHESSI
AB Extreme ultraviolet (EUV) images of solar flares provided by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) are often affected by saturation effects in their core, physically most interesting, region. We introduce an image reconstruction procedure that allows recovering information in the primary saturation domain using the secondary images produced by the diffraction fringes as input data. Such a procedure is based on standard image-processing tools like correlation, convolution, and back-projection. Its effectiveness is tested in the case of AIA/SDO observations of the 2013 July 8 flaring event.
C1 [Schwartz, R. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Schwartz, R. A.] Catholic Univ Amer, Greenbelt, MD 20771 USA.
   [Torre, G.; Piana, M.] Univ Genoa, Dipartimento Matemat, I-16146 Genoa, Italy.
   [Torre, G.; Piana, M.] CNR SPIN, I-16146 Genoa, Italy.
RP Schwartz, RA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM richard.a.schwartz@nasa.gov; torre@dima.unige.it; piana@dima.unige.it
RI piana, michele/H-9376-2015; 
OI PIANA, MICHELE/0000-0003-1700-991X
FU NASA grant [NNX14AG06G]; RHESSI funds [NNX11AB37G]
FX R.S. was supported by NASA grant NNX14AG06G. G.T. was supported during
   his stay at Goddard by the Catholic University of America in Washington,
   DC, using RHESSI funds under grant number NNX11AB37G. Anna Maria Massone
   and Federico Benvenuto are kindly acknowledged for fruitful discussions.
NR 12
TC 5
Z9 5
U1 1
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 OCT 1
PY 2014
VL 793
IS 2
AR L23
DI 10.1088/2041-8205/793/2/L23
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP2ES
UT WOS:000341885900002
ER

PT J
AU Strohmayer, T
   Mahmoodifar, S
AF Strohmayer, Tod
   Mahmoodifar, Simin
TI DISCOVERY OF A NEUTRON STAR OSCILLATION MODE DURING A SUPERBURST
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE methods: data analysis; stars: neutron; stars: oscillations; stars:
   rotation; X-rays: binaries; X-rays: individual (4U 1636-536)
ID X-RAY BINARIES; R-MODE; MILLISECOND PULSAR; XTE J1751-305; LIGHT CURVES;
   4U 1636-536; MASS; INSTABILITY; MODULATION; EXCITATION
AB Neutron stars are among the most compact objects in the universe and provide a unique laboratory for the study of cold ultra-dense matter. While asteroseismology can provide a powerful probe of the interiors of stars, for example, helioseismology has provided unprecedented insights about the interior of the Sun, comparable capabilities for neutron star seismology have not yet been achieved. Here, we report the discovery of a coherent X-ray modulation from the neutron star 4U 1636-536 during the 2001 February 22 thermonuclear superburst seen with NASA's Rossi X-Ray Timing Explorer (RXTE) that is very likely produced by a global oscillation mode. The observed frequency is 835.6440 +/- 0.0002 Hz (1.43546 times the stellar spin frequency of 582.14323 Hz) and the modulation is well described by a sinusoid (A + B sin(phi - phi(0))) with a fractional half-amplitude of B/A = 0.19 +/- 0.04% (4-15 keV). The observed frequency is consistent with the expected inertial frame frequency of a rotationally modified surface g-mode, an interfacial mode in the ocean-crust interface, or perhaps an r-mode. Observing an inertial frame frequency-as opposed to a co-rotating frame frequency-appears consistent with the superburst's thermal emission arising from the entire surface of the neutron star, and the mode may become visible by perturbing the local surface temperature. We briefly discuss the implications of the mode detection for the neutron star's projected velocity and mass. Our results provide further strong evidence that global oscillation modes can produce observable modulations in the X-ray flux from neutron stars.
C1 [Strohmayer, Tod] NASAs Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
   [Strohmayer, Tod] NASAs Goddard Space Flight Ctr, Joint Space Sci Inst, Greenbelt, MD 20771 USA.
   [Mahmoodifar, Simin] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
   [Mahmoodifar, Simin] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
RP Strohmayer, T (reprint author), NASAs Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
FU U.S. Department of Energy [DEFG02-93ER-40762]
FX We thank Cole Miller, Tony Piro, and the anonymous referee for helpful
   comments and discussions. T.S. acknowledges NASA's support for
   high-energy astrophysics. S.M. acknowledges the support of the U.S.
   Department of Energy through grant number DEFG02-93ER-40762.
NR 34
TC 7
Z9 7
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 1
PY 2014
VL 793
IS 2
AR L38
DI 10.1088/2041-8205/793/2/L38
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP2ES
UT WOS:000341885900017
ER

PT J
AU Wang, LH
   Li, G
   Shih, AY
   Lin, RP
   Wimmer-Schweingruber, RF
AF Wang, Linghua
   Li, Gang
   Shih, Albert Y.
   Lin, Robert P.
   Wimmer-Schweingruber, Robert F.
TI SIMULATION OF ENERGETIC NEUTRAL ATOMS FROM SOLAR ENERGETIC PARTICLES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE acceleration of particles; Sun: coronal mass ejections (CMEs); Sun:
   particle emission
ID HYDROMAGNETIC WAVE EXCITATION; HYDROGEN-ATOMS; INTERPLANETARY SHOCKS;
   ION-ACCELERATION; ELECTRON-CAPTURE; DECEMBER 5; HELIOSPHERE; WIND; ACE;
   PROTONS
AB Energetic neutral atoms (ENAs) provide the only way to observe the acceleration site of coronal-mass-ejection-driven (CME-driven) shock-accelerated solar energetic particles (SEPs). In gradual SEP events, energetic protons can charge exchange with the ambient solar wind or interstellar neutrals to become ENAs. Assuming a CME-driven shock with a constant speed of 1800 km s(-1) and compression ratio of 3.5, propagating from 1.5 to 40 R-S, we calculate the accelerated SEPs at 5-5000 keV and the resulting ENAs via various charge-exchange interactions. Taking into account the ENA losses in the interplanetary medium, we obtain the flux-time profiles of these solar ENAs reaching 1 AU. We find that the arriving ENAs at energies above similar to 100 keV show a sharply peaked flux-time profile, mainly originating from the shock source below 5 R-S, whereas the ENAs below similar to 20 keV have a flat-top time profile, mostly originating from the source beyond 10 R-S. Assuming the accelerated protons are effectively trapped downstream of the shock, we can reproduce the STEREO ENA fluence observations at similar to 2-5MeV/nucleon. We also estimate the flux of ENAs coming from the charge exchange of energetic storm protons, accelerated by the fast CME-driven shock near 1 AU, with interstellar hydrogen and helium. Our results suggest that appropriate instrumentation would be able to detect ENAs from SEPs and to even make ENA images of SEPs at energies above similar to 10-20 keV.
C1 [Wang, Linghua] Peking Univ, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China.
   [Li, Gang] Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA.
   [Li, Gang] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
   [Shih, Albert Y.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA.
   [Lin, Robert P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Wimmer-Schweingruber, Robert F.] Univ Kiel, Inst Expt & Angew Phys, D-24118 Kiel, Germany.
RP Wang, LH (reprint author), Peking Univ, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China.
EM wanglhwang@gmail.com
RI Wang, Linghua/C-4938-2014
OI Wang, Linghua/0000-0001-7309-4325
FU NSFC [41274172, 41474148, 41421003]; NSF grants [M-0847719,
   AGS-1135432]; Goddard Internal Research and Development (IRAD) program;
   German Space Agency, DLR [50 OT 1202]
FX We thank R. P. Lin for his inspiration, wisdom, perpetual enthusiasm,
   and love of science. This research at Peking University was supported in
   part by NSFC under contract 41274172, 41474148, and 41421003. G. Li was
   supported by NSF grants ATM-0847719 and AGS-1135432. A. Shih was
   supported by funding from the Goddard Internal Research and Development
   (IRAD) program. R. Wimmer-Schweingruber thanks the German Space Agency,
   DLR, for their strong support of the Solar Orbiter under contract 50 OT
   1202.
NR 34
TC 1
Z9 1
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 1
PY 2014
VL 793
IS 2
AR L37
DI 10.1088/2041-8205/793/2/L37
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AP2ES
UT WOS:000341885900016
ER

PT J
AU Broschart, SB
   Lantoine, G
   Grebow, DJ
AF Broschart, Stephen B.
   Lantoine, Gregory
   Grebow, Daniel J.
TI Quasi-terminator orbits near primitive bodies
SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY
LA English
DT Article
DE Hamiltonian systems; Restricted problems; Periodic orbits; Asteroid;
   Solar radiation pressure; Quasi-periodic motion
ID SATELLITE DYNAMICS; RADIATION PRESSURE; ASTEROIDS; SHAPE; STABILITY;
   COMET
AB Quasi-terminator orbits are introduced as a class of quasi-periodic trajectories in the solar radiation pressure (SRP) perturbed Hill dynamics. These orbits offer significant displacements along the Sun-direction without the need for station-keeping maneuvers. Thus, quasi-terminator orbits have application to primitive-body mapping missions, where a variety of observation geometries relative to the Sun (or other directions) can be achieved. This paper describes the characteristics of these orbits as a function of normalized SRP strength and invariant torus frequencies and presents a discussion of mission design considerations for a global surface mapping orbit design.
C1 [Broschart, Stephen B.; Lantoine, Gregory; Grebow, Daniel J.] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Pasadena, CA 91109 USA.
RP Broschart, SB (reprint author), CALTECH, Jet Prop Lab, Mission Design & Nav Sect, M-S 301-121,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Stephen.B.Broschart@jpl.nasa.gov
NR 31
TC 8
Z9 8
U1 0
U2 1
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 OCT
PY 2014
VL 120
IS 2
BP 195
EP 215
DI 10.1007/s10569-014-9574-3
PG 21
WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications
SC Astronomy & Astrophysics; Mathematics
GA AP1VK
UT WOS:000341859800004
ER

PT J
AU Zhang, M
   Konishi, H
   Xu, HF
   Sun, XM
   Lu, HF
   Wu, DD
   Wu, NY
AF Zhang, Mei
   Konishi, Hiromi
   Xu, Huifang
   Sun, Xiaoming
   Lu, Hongfeng
   Wu, Daidai
   Wu, Nengyou
TI Morphology and formation mechanism of pyrite induced by the anaerobic
   oxidation of methane from the continental slope of the NE South China
   Sea
SO JOURNAL OF ASIAN EARTH SCIENCES
LA English
DT Article
DE Pyrite; Marcasite; Spherule; Framboid; Anaerobic oxidation of methane;
   AOM; South China Sea
ID GULF-OF-MEXICO; SULFIDE MINERAL FORMATION; GAS HYDRATE OCCURRENCE;
   SULFATE REDUCTION; SEEP CARBONATES; AUTHIGENIC CARBONATES; FRAMBOIDAL
   PYRITE; MARINE-SEDIMENTS; REDOX CONDITIONS; BARITE DEPOSITS
AB In order to understand the response of authigenic pyrite to gas hydrate geo-systems, pyrite tubes or rods at the sulfate methane transition (SMT) zone of cord GC10 from the northern continental slope of the South China Sea (SCS) were investigated. In situ X-ray diffraction (XRD) results show that the pyrite tube consists of pyrite micro-crystals with trace amount of graphite in the inner tube. Scanning electron microscope (SEM) observations of pyrite tubes indicate various aggregations in the form of framboidal, euhedral, and colloidal pyrite microcrystals. Typical framboidal pyrite is considered as packing of octahedral microcrystals. Interestingly, many framboids in the tubes consist of round or irregular microcrystals and have an outer crust that consists of secondary pyrite. The size of the framboids in the inner wall of the tube is larger than that in the middle wall or foraminifer-filled pyrite. High-resolution transmission electron microscopic (HRTEM) images show marcasite lamellae defects in the spherulitic pyrite crystals, which reveal different solution conditions during the pyrite precipitation. Nano-foil-like graphitic carbon was observed to be closely associated with the pyrite spherules. The occurrence of both marcasite layers and nano-foil-like graphitic carbon suggest that the migration of methane from deep sediment. It is suggested that the formation of pyrite serves as a catalyst during the reaction from methane to elemental carbon under the anaerobic oxidation of methane. Meanwhile, this reaction results in local acidification of the solution inside the pyrite tubes, which favors marcasite lamellae growth on the host pyrite substrate. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Zhang, Mei; Wu, Daidai; Wu, Nengyou] Chinese Acad Sci, Guangzhou Inst Energy Convers, Guangzhou 510640, Guangdong, Peoples R China.
   [Zhang, Mei; Konishi, Hiromi; Xu, Huifang] Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA.
   [Zhang, Mei; Sun, Xiaoming] Sun Yat Sen Univ, Sch Earth Sci & Geol Engn, Guangzhou 510275, Guangdong, Peoples R China.
   [Sun, Xiaoming] Sun Yat Sen Univ, Sch Marine Sci, Guangzhou 510006, Guangdong, Peoples R China.
   [Sun, Xiaoming] Key Lab Marine Resources & Coastal Engn Guangdong, Guangzhou 510275, Guangdong, Peoples R China.
   [Lu, Hongfeng] Guangzhou Marine Geol Survey, Guangzhou 510760, Guangdong, Peoples R China.
RP Zhang, M (reprint author), Chinese Acad Sci, Guangzhou Inst Energy Convers, Guangzhou 510640, Guangdong, Peoples R China.
EM zhangmei@ms.giec.ac.cn; hfxu@geology.wisc.edu
FU Natural Science Foundation of China [41306061, 41273022, 91128101];
   Natural Science Foundation of Guangdong Province, China
   [S2012040007118]; NASA Astrobiology Institute [N07-5489]; Guangdong
   Province Universities and Colleges Pearl River Scholar Funded Scheme;
   National 127 project
FX This work was supported by Natural Science Foundation of China (Nos.
   41306061, 41273022 and 91128101), the Natural Science Foundation of
   Guangdong Province, China (No. S2012040007118), NASA Astrobiology
   Institute (N07-5489), and Guangdong Province Universities and Colleges
   Pearl River Scholar Funded Scheme (2011) and National 127 project.
   Furthermore, we thank Nick Levitt, two anonymous reviewers, and the
   editor for their helpful comments that greatly improved an earlier
   version of this manuscript.
NR 67
TC 7
Z9 7
U1 9
U2 62
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1367-9120
EI 1878-5786
J9 J ASIAN EARTH SCI
JI J. Asian Earth Sci.
PD OCT 1
PY 2014
VL 92
SI SI
BP 293
EP 301
DI 10.1016/j.jseaes.2014.05.004
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA AO7SY
UT WOS:000341554100021
ER

PT J
AU Balbin, R
   Lopez-Jurado, JL
   Flexas, MM
   Reglero, P
   Velez-Velchi, P
   Gonzalez-Pola, C
   Rodriguez, JM
   Garcia, A
   Alemany, F
AF Balbin, R.
   Lopez-Jurado, J. L.
   Flexas, M. M.
   Reglero, P.
   Velez-Velchi, P.
   Gonzalez-Pola, C.
   Rodriguez, J. M.
   Garcia, A.
   Alemany, F.
TI Interannual variability of the early summer circulation around the
   Balearic Islands: Driving factors and potential effects on the marine
   ecosystem
SO JOURNAL OF MARINE SYSTEMS
LA English
DT Article; Proceedings Paper
CT International Workshop on Environment, Ecosystems and Demersal Resources
   and Fisheries
CY NOV 14-16, 2012
CL Palma de Mallorca, SPAIN
DE Ocean circulation; Oceanic fronts; Water masses; Western Mediterranean
   Sea; Balearic Sea; Regional climatic index
ID WINTER INTERMEDIATE WATERS; MEDITERRANEAN-SEA; FISH; FRONT; BASIN;
   PROJECT; LARVAE
AB Six summer surveys conducted from 2001 to 2005 and in 2012 by the Spanish Institute of Oceanography (IEO) reveal that the hydrographic early summer scenarios around the Balearic Islands are related to the winter atmospheric forcing in the northwestern Mediterranean Sea. The Balearic Islands (western Mediterranean Sea) lie at the transition between the southern, fresher, newly arrived Atlantic Waters (AWs) and the northern, saltier, resident AW. The meridional position of the salinity driven oceanic density front separating the new from the resident AW is determined by the presence/absence of Western Intermediate Water (WON) in the Mallorca and Ibiza channels. When WON is present in the channels, the oceanic density front is found either at the south of the islands, or along the Emile Baudot escarpment In contrast, when WON is absent, new AW progresses northwards crossing the Ibiza channel and/or the Mallorca channel. In this later scenario, the oceanic density front is closer to the Balearic Islands. A good correspondence exists between standardized winter air temperature anomaly in the Gulf of Lions and the presence of WIW in the channels. We discuss the use of a regional climatic index based on these parameters to forecast in a first-order approach the position of the oceanic front, as it is expected to have high impact on the regional marine ecosystem. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Balbin, R.; Lopez-Jurado, J. L.; Reglero, P.; Alemany, F.] Ctr Oceanog Balears, Inst Espanol Oceanog, Palma De Mallorca 07015, Spain.
   [Gonzalez-Pola, C.; Rodriguez, J. M.] Ctr Oceanog Santander, Inst Espanol Oceanog, Malaga, Spain.
   [Velez-Velchi, P.] Ctr Oceanog Canarias, Inst Espanol Oceanog, Las Palmas Gran Canaria, Spain.
   [Garcia, A.] Ctr Oceanog Malaga, Inst Espanol Oceanog, Malaga, Spain.
   [Flexas, M. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Balbin, R (reprint author), Ctr Oceanog Balears, Inst Espanol Oceanog, Muelle de Poniente S-N, Palma De Mallorca 07015, Spain.
EM rosa.balbin@ba.ieo.es
RI Rodriguez, Jose /L-1576-2014; Balbin, Rosa/F-8210-2010; 
OI Rodriguez, Jose /0000-0001-7702-5407; Balbin, Rosa/0000-0001-5231-1300;
   Alemany, F. (Francisco)/0000-0001-6265-5545
NR 44
TC 15
Z9 15
U1 2
U2 16
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0924-7963
EI 1879-1573
J9 J MARINE SYST
JI J. Mar. Syst.
PD OCT
PY 2014
VL 138
SI SI
BP 70
EP 81
DI 10.1016/j.jmarsys.2013.07.004
PG 12
WC Geosciences, Multidisciplinary; Marine & Freshwater Biology;
   Oceanography
SC Geology; Marine & Freshwater Biology; Oceanography
GA AO6OR
UT WOS:000341471900008
ER

PT J
AU Howar, F
   Isberner, M
   Merten, M
   Steffen, B
   Beyer, D
   Pasareanu, CS
AF Howar, Falk
   Isberner, Malte
   Merten, Maik
   Steffen, Bernhard
   Beyer, Dirk
   Pasareanu, Corina S.
TI Rigorous examination of reactive systems The RERS challenges 2012 and
   2013
SO INTERNATIONAL JOURNAL ON SOFTWARE TOOLS FOR TECHNOLOGY TRANSFER
LA English
DT Editorial Material
DE Program analysis; Model checking; Verification; Model-based testing;
   Competition; Reactive system; Event-condition-action system
AB The goal of the RERS challenge is to evaluate the effectiveness of various verification and validation approaches on reactive systems, a class of systems that is highly relevant for industrial critical applications. The RERS challenge brings together researchers from different areas of software verification and validation, including static analysis, model checking, theorem proving, symbolic execution, and testing. The challenge provides a forum for experimental comparison of different techniques on specifically designed verification tasks. These benchmarks are automatically synthesized to exhibit chosen properties, and then enhanced to include dedicated dimensions of difficulty, such as conceptual complexity of the properties (e.g., reachability, safety, liveness), size of the reactive systems (a few hundred lines to millions of lines), and complexity of language features (arrays and pointer arithmetic). The STTT special section on RERS describes the results of the evaluations and the different analysis techniques that were used in the RERS challenges 2012 and 2013.
C1 [Howar, Falk; Pasareanu, Corina S.] NASA Ames, Carnegie Mellon Silicon Valley, Mountain View, CA USA.
   [Isberner, Malte; Merten, Maik; Steffen, Bernhard] TU Dortmund, Dortmund, Germany.
   [Beyer, Dirk] Univ Passau, D-94032 Passau, Germany.
RP Isberner, M (reprint author), TU Dortmund, Dortmund, Germany.
EM malte.isberner@cs.uni-dortmund.de
NR 40
TC 1
Z9 1
U1 0
U2 0
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1433-2779
EI 1433-2787
J9 INT J SOFTW TOOLS TE
JI Int. J. Softw. Tools Technol. Transf.
PD OCT
PY 2014
VL 16
IS 5
BP 457
EP 464
DI 10.1007/s10009-014-0337-y
PG 8
WC Computer Science, Software Engineering
SC Computer Science
GA V43HU
UT WOS:000209673300001
ER

PT J
AU Stephens, DB
   Verdugo, FR
   Bennett, GJ
AF Stephens, David B.
   Verdugo, Francisco R.
   Bennett, Gareth J.
TI Shear Layer Driven Acoustic Modes in a Cylindrical Cavity
SO JOURNAL OF PRESSURE VESSEL TECHNOLOGY-TRANSACTIONS OF THE ASME
LA English
DT Article
ID FLOW
AB This paper describes the interior acoustic pressure of a cylindrical cavity driven by a shear layer. Existing cavity flow literature is generally focused on rectangular cavities, where the resonance is either longitudinal or the result of excited depth modes inside the cavity. The design of the present circular cavity is such that azimuthal duct modes can be excited in various combinations with depth modes depending on free stream velocity. An acoustic simulation of the system was used to identify the modes as a function of frequency when the system is driven by an acoustic point source. With appropriate manipulation of the free stream flow, abrupt mode switching and mode oscillation were both observed, and a condition with a dominant azimuthal mode was found. The strength of the lock-on was documented for the various resonance conditions, and the effects of the cavity opening size and location were studied.
C1 [Stephens, David B.] NASA, Glenn Res Ctr, Cleveland, OH 44070 USA.
   [Verdugo, Francisco R.] Univ Roma Tre, Dipartimento Ingn Meccan & Ind, I-00146 Rome 79, Italy.
   [Bennett, Gareth J.] Trinity Coll Dublin, Dept Mech & Mfg Engn, Dublin 2, Ireland.
RP Bennett, GJ (reprint author), Trinity Coll Dublin, Dept Mech & Mfg Engn, Dublin 2, Ireland.
EM gareth.bennett@tcd.ie
FU Erasmus Mundus Master of Mechanical Engineering program
FX The authors would like to thank the Erasmus Mundus Master of Mechanical
   Engineering program for visiting scholars for financially supporting Dr.
   Stephens and his contribution to this work at Trinity College Dublin.
NR 17
TC 1
Z9 1
U1 0
U2 3
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0094-9930
EI 1528-8978
J9 J PRESS VESS-T ASME
JI J. Press. Vessel Technol.-Trans. ASME
PD OCT
PY 2014
VL 136
IS 5
AR 051309
DI 10.1115/1.4026866
PG 8
WC Engineering, Mechanical
SC Engineering
GA AO6UJ
UT WOS:000341486900010
ER

PT J
AU Jenson, RM
   Wollman, AP
   Weislogel, MM
   Sharp, L
   Green, R
   Canfield, PJ
   Klatte, J
   Dreyer, ME
AF Jenson, Ryan M.
   Wollman, Andrew P.
   Weislogel, Mark M.
   Sharp, Lauren
   Green, Robert
   Canfield, Peter J.
   Klatte, Joerg
   Dreyer, Michael E.
TI Passive phase separation of microgravity bubbly flows using conduit
   geometry
SO INTERNATIONAL JOURNAL OF MULTIPHASE FLOW
LA English
DT Article
DE Two-phase flow; Capillary fluidics; Microfluidics; Passive phase
   separations; Microgravity; Spacecraft
ID CAPILLARY-FLOW; CHANNEL; MICROCHANNELS; BEHAVIOR; SURFACE; DESIGN
AB The ability to separate liquid and gas phases in the absence of a gravitational acceleration has proven a challenge to engineers since the inception of space exploration. Due to our singular experience with terrestrial systems, artificial body forces are often imparted in multiphase fluid systems aboard spacecraft to reproduce the buoyancy effect. This approach tends to be inefficient, adding complexity, resources, and failure modes. Ever present in multiphase phenomena, the forces of surface tension can be exploited to aid passive phase separations where performance characteristics are determined solely by geometric design and system wettability. Said systems may be readily designed as demonstrated herein where a regulated bubbly flow is drawn through an open triangular sectioned duct. The bubbles passively migrate toward the free surface where they coalesce and leave the flow. The tests clearly show container aspect ratios required for passive phase separations for various liquid and gas flow rates. Preliminary data are presented as regime maps demarking complete phase separation. Long duration microgravity experiments are performed aboard the International Space Station. Supplementary experiments are conducted ;using a drop tower. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Jenson, Ryan M.] IRPI LLC, Wilsonville, OR 97070 USA.
   [Wollman, Andrew P.; Weislogel, Mark M.] Portland State Univ, Dept Mech & Mat Engn, Portland, OR 97201 USA.
   [Sharp, Lauren; Green, Robert] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
   [Canfield, Peter J.; Klatte, Joerg; Dreyer, Michael E.] Ctr Appl Space Technol & Micrograv, D-28359 Bremen, Germany.
RP Weislogel, MM (reprint author), Portland State Univ, Dept Mech & Mat Engn, 1930 SW 4th Ave, Portland, OR 97201 USA.
EM mwei@pdx.edu
FU National Aeronautics and Space Agency [NNX09AP66A]; German Federal
   Ministry of Economics and Technology (BMWi) via the German Aerospace
   Center (DLR) [50WM1145]; NASA/Oregon Space Grant Consortium [NNX10AK68H]
FX Support for this work is shared by the National Aeronautics and Space
   Agency cooperative agreement NNX09AP66A and the German Federal Ministry
   of Economics and Technology (BMWi) via the German Aerospace Center (DLR)
   under Grant No. 50WM1145. We wish to thank astronaut Mike Fossum, PSU
   graduate student Will Blackmore, Astrium Engineering, and the NASA cadre
   at Glenn Research Center, Johnson Space Center, and especially the MSG
   crew at Marshall Spaceflight Center for support during the flight
   operations. A.P. Wollman is supported in part through NASA/Oregon Space
   Grant Consortium grant NNX10AK68H.
NR 33
TC 1
Z9 1
U1 7
U2 33
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0301-9322
EI 1879-3533
J9 INT J MULTIPHAS FLOW
JI Int. J. Multiph. Flow
PD OCT
PY 2014
VL 65
BP 68
EP 81
DI 10.1016/j.ijmultiphaseflow.2014.05.011
PG 14
WC Mechanics
SC Mechanics
GA AO4VP
UT WOS:000341339800008
ER

PT J
AU Rai, MM
AF Rai, Man Mohan
TI Flow phenomena in the very near wake of a flat plate with a circular
   trailing edge
SO JOURNAL OF FLUID MECHANICS
LA English
DT Article
DE turbulence simulation; vortex shedding; wakes/jets
ID DIRECT NUMERICAL-SIMULATION; BLUFF-BODY; CYLINDER; TURBULENT;
   INSTABILITY; PRESSURE; DRAG
AB The very near wake of a flat plate with a circular trailing edge, exhibiting pronounced shedding of wake vortices, is investigated with data from direct numerical simulations (DNSs). Computations were performed for two cases. In the first case the Reynolds numbers based on plate length and thickness were 1.255 x 10(6) and 1.0 x 10(4), respectively. In the second case the two Reynolds numbers were 3.025 x 10(5) and 5.0 x 10(3), respectively. The separating boundary layers are turbulent and statistically identical thus resulting in a wake that is symmetric in the mean. The focus here is on the instability of the detached shear layers and the evolution of rib-vortex-induced localized regions of reverse flow. These regions detach from the main body of reverse flow in the trailing edge region and are convected downstream. The detached shear layers intermittently exhibit unstable behaviour, sometimes resulting in the development of shear-layer vortices as seen in earlier cylinder flow investigations with laminar separating boundary layers. Only a small fraction of the separated turbulent boundary layer experiences this instability, and also rolls up into the initial shed vortices. The instability causes a broadband peak in pressure spectra computed within the shear layers. Phase-averaged intensity and shear stress distributions of the randomly fluctuating component of velocity in the very near wake are also provided here and compared with those obtained in the near wake. The distributions of the production terms in the transport equations for the turbulent stresses are also provided.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Rai, MM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM man.m.rai@nasa.gov
NR 18
TC 1
Z9 1
U1 2
U2 18
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 OCT
PY 2014
VL 756
BP 510
EP 543
DI 10.1017/jfm.2014.466
PG 34
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA AO2FA
UT WOS:000341130000022
ER

PT J
AU Tewari, SN
   Grugel, RN
   Poirier, DR
AF Tewari, S. N.
   Grugel, R. N.
   Poirier, D. R.
TI An Evaluation of Primary Dendrite Trunk Diameters in Directionally
   Solidified Al-Si Alloys
SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND
   MATERIALS SCIENCE
LA English
DT Article
ID ARRAY GROWTH; STRUCTURE PREDICTIONS; STABILITY
AB The primary dendrite trunk diameters of Al-Si alloys that were directionally solidified over a range of processing conditions have been evaluated. The empirical data are analyzed with a model that is an extension of one used to describe the ripening of dendrite arms. The analysis, based primarily on an assessment of secondary dendrite arm dissolution in the mushy zone, fits well with the experimental data. It is suggested that the primary dendrite trunk diameter is a useful metric that correlates well with the actual solidification processing parameters, and complements the conventionally used primary, secondary, and tertiary arm spacings.
C1 [Tewari, S. N.] Cleveland State Univ, Dept Chem & Biomed Engn, Cleveland, OH 44115 USA.
   [Grugel, R. N.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
   [Poirier, D. R.] Univ Arizona, Dept Mat Sci & Engn, Tucson, AZ 85721 USA.
RP Grugel, RN (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM Richard.n.grugel@nasa.gov
FU NASA [NNX08AN49G]; NASA Microgravity Materials Science program
FX The authors appreciate and acknowledge the support provided by NASA
   Grant NNX08AN49G, and the NASA Microgravity Materials Science program.
   One of the authors (RNG) wishes to acknowledge Professor W. Kurz of the
   Ecole Polytechnique Federal de Lausanne for the time in his laboratory
   which generated the data shown in Figures 5 and 6.
NR 24
TC 2
Z9 2
U1 1
U2 5
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1073-5623
EI 1543-1940
J9 METALL MATER TRANS A
JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci.
PD OCT
PY 2014
VL 45A
IS 11
BP 4758
EP 4761
DI 10.1007/s11661-014-2438-3
PG 4
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
   Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA AO1PY
UT WOS:000341086700007
ER

PT J
AU Lee, H
   Park, I
   Mudawar, I
   Hasan, MM
AF Lee, Hyoungsoon
   Park, Ilchung
   Mudawar, Issam
   Hasan, Mohammad M.
TI Micro-channel evaporator for space applications-1. Experimental pressure
   drop and heat transfer results for different orientations in earth
   gravity
SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER
LA English
DT Article
DE Flow boiling; Micro-channel; Pressure drop; Flow orientation; Reduced
   gravity
ID FLOW BOILING CHF; RECTANGULAR CHANNEL; SINGLE-PHASE; FLUOROCARBON
   LIQUID; HORIZONTAL TUBES; 2-PHASE INLET; BODY FORCE; WATER-FLOW; FLUX
   CHF; CONDENSATION
AB Boiling and condensation are being considered for operation of thermal control systems (TCSs) in future space vehicles to capitalize upon their high heat transfer coefficients and appreciable reduction in TCS weight and volume. A primary concern in designing these systems is a lack of technical knowhow on the influence of buoyancy and therefore body force on two-phase heat transfer in reduced gravity. In particular, there is keen interest in developing predictive tools for pressure drop and heat transfer and identifying the minimum coolant flow rate that would negate the influence of body force. Two-phase flow in micro-channels provides unique advantages to space systems by greatly increasing flow inertia for a given flow rate, which helps resist body forces effects. This study is the first part of a two-part study addressing the effectiveness of two-phase micro-channels at negating body force effects. Flow boiling experiments are conducted with FC-72 in a test module containing 80 of 231 mu m wide x 1000 mu m deep micro-channels in three different flow orientations: horizontal, vertical upflow and vertical downflow over broad ranges of mass velocity and heat flux. Also investigated are conditions that trigger two different types of two-phase flow instability. In addition, different flow regimes are identified with an aid of high-speed video imaging, and the flow regime data are compared to an exiting flow regime map and used to develop new relations for transition boundaries between regimes. Overall, the present study proves the existence of a mass velocity threshold above which identical heat transfer performances are achieved regardless of orientations. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Lee, Hyoungsoon; Park, Ilchung; Mudawar, Issam] PU BTPFL, Sch Mech Engn, W Lafayette, IN 47907 USA.
   [Hasan, Mohammad M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Mudawar, I (reprint author), PU BTPFL, Sch Mech Engn, 585 Purdue Mall, W Lafayette, IN 47907 USA.
EM mudawar@ecn.purdue.edu
FU National Aeronautics and Space Administration (NASA) - United States
   [NNX13AC83G]
FX The authors are grateful for the support of the National Aeronautics and
   Space Administration (NASA) - United States under Grant no. NNX13AC83G.
NR 55
TC 8
Z9 10
U1 1
U2 24
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 2014
VL 77
BP 1213
EP 1230
DI 10.1016/j.ijheatmasstransfer.2014.06.012
PG 18
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA AN0VP
UT WOS:000340302400110
ER

PT J
AU Lee, H
   Park, I
   Mudawar, I
   Hasan, MM
AF Lee, Hyoungsoon
   Park, Ilchung
   Mudawar, Issam
   Hasan, Mohammad M.
TI Micro-channel evaporator for space applications-2. Assessment of
   predictive tools
SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER
LA English
DT Article
DE Flow boiling; Micro-channel; Pressure drop; Flow orientation; Reduced
   gravity
ID CRITICAL HEAT-FLUX; FRICTIONAL PRESSURE-DROP; FLOW BOILING CHF; 2-PHASE
   FLOW; SINGLE-PHASE; GENERAL CORRELATION; MICRO/MINI-CHANNELS; TRANSFER
   COEFFICIENT; UNIVERSAL APPROACH; HORIZONTAL TUBE
AB This study is the second part of a two-part study addressing the effectiveness of micro-channel evaporators for space applications. The first part provided pressure drop and heat transfer data for FC-72 that were acquired with a test module containing 80 of 231 mu m wide x 1000 mu m deep micro-channels. The tests were performed in three flow orientations: horizontal, vertical upflow and vertical downflow over broad ranges of mass velocity and heat flux. The present part uses these experimental results to assess the accuracy of published predictive tools. The two-phase heat transfer coefficient data are compared to predictions of 15 popular correlations, and pressure drop data to 7 mixture viscosity relations used in conjunction of the Homogeneous Equilibrium Model (HEM), and 18 correlations based on the Separated Flow Model (SFM). These models and correlations are carefully assessed in pursuit of identifying the most accurate tools. In addition, three important criteria for implementing micro-channel flow boiling in space systems are proposed: avoiding large pressure drop, avoiding critical heat flux (CHF), and negating the influence of body force. It is shown that micro-channels require significantly smaller mass velocities to negate body force effects than macro-channels, and are therefore very effective for space applications. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Lee, Hyoungsoon; Park, Ilchung; Mudawar, Issam] Purdue Univ, Sch Mech Engn, BTPFL, W Lafayette, IN 47907 USA.
   [Hasan, Mohammad M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Mudawar, I (reprint author), Purdue Univ, Sch Mech Engn, BTPFL, 585 Purdue Mall, W Lafayette, IN 47907 USA.
EM mudawar@ecn.purdue.edu
FU National Aeronautics and Space Administration (NASA) - United States
   [NNX13AC83G]
FX The authors are grateful for the support of the National Aeronautics and
   Space Administration (NASA) - United States under Grant No. NNX13AC83G.
NR 78
TC 4
Z9 6
U1 2
U2 13
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 2014
VL 77
BP 1231
EP 1249
DI 10.1016/j.ijheatmasstransfer.2014.06.008
PG 19
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA AN0VP
UT WOS:000340302400111
ER

PT J
AU Loftus, AM
   Cotton, WR
AF Loftus, A. M.
   Cotton, W. R.
TI Examination of CCN impacts on hail in a simulated supercell storm with
   triple-moment hail bulk microphysics
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Hail; CCN; Supercell convection; Aerosol-cloud-precipitation
   interactions; Cloud-resolving model
ID DEEP CONVECTIVE CLOUDS; VERTICAL WIND SHEAR; PART I; HAILSTONE GROWTH;
   CUMULUS CLOUD; NUMERICAL-SIMULATION; HIGH-PLAINS; ATMOSPHERIC AEROSOLS;
   CONDENSATION NUCLEI; NUCLEATING AEROSOL
AB Aerosols that act as cloud condensation nuclei (CCN) play a crucial role in the formation of cloud particles and recent research suggests that CCN can influence ice processes within deep convection as well. In this study, a triple-moment bulk hail microphysics scheme is used to investigate the impact of changing CCN concentrations on hail for a well-observed supercell storm that occurred over northwest Kansas on 29 June 2000 during the Severe Thunderstorm and Electrification and Precipitation Study (STEPS). For the simulated supercells in the particular environment examined, an increase in potential CCN concentrations from 100 to 3000 cm(-3) leads to increasing numbers and decreasing sizes of cloud droplets, as expected, yet the overall storm dynamics and evolution are largely unaffected. Increases in potential CCN concentrations lead to non-monotonic responses in the bulk characteristics of nearly all hydrometeor fields, surface precipitation, and cold-pool strength. However, higher concentrations of CCN also result in larger hail sizes and greater amounts of large diameter (>= 2 cm) hail. The results suggest that a combination of increased sizes and localized reductions in numbers of hail embryos near favorable growth regions with increasing potential CCN concentrations tend to promote conditions that lead to increased hail sizes and amounts of large hail. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Loftus, A. M.; Cotton, W. R.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
RP Loftus, AM (reprint author), NASA, Goddard Space Flight Ctr, Climate & Radiat & Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM adrian.m.loftus@nasa.gov
FU NSF grants [ATM-0324324, ATM-0638910, AGS-1005041]
FX The authors wish to thank J. Milbrandt and one anonymous reviewer for
   their suggestion on improving this manuscript. This research was
   supported by NSF grants ATM-0324324, ATM-0638910, and AGS-1005041.
NR 107
TC 11
Z9 11
U1 1
U2 9
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 2014
VL 147
BP 183
EP 204
DI 10.1016/j.atmosres.2014.04.017
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AN0VZ
UT WOS:000340303400015
ER

PT J
AU Robertson, S
   Dickson, S
   Horanyi, M
   Sternovsky, Z
   Friedrich, M
   Janches, D
   Megner, L
   Williams, B
AF Robertson, Scott
   Dickson, Shannon
   Horanyi, Mihaly
   Sternovsky, Zoltan
   Friedrich, Martin
   Janches, Diego
   Megner, Linda
   Williams, Bifford
TI Detection of meteoric smoke particles in the mesosphere by a
   rocket-borne mass spectrometer
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Mesosphere; Charged MSPs; In situ data; Mass spectrometer
ID DESCRIBING AEROSOL FORMATION; POLAR SUMMER MESOSPHERE; DUST PARTICLES;
   ICE PARTICLES; CHARGED DUST; D-REGION; DIFFERENTIAL ABSORPTION;
   ELECTRON-DENSITY; FARADAY-ROTATION; SOUNDING ROCKET
AB In October 2011, two CHAMPS (Charge And Mass of meteoric smoke ParticleS) sounding rockets were launched into the polar mesosphere, each carrying an electrostatic multichannel mass analyzer for charged meteoric smoke particles (MSPs) that operated from 60 to 100 km and returned data on the number density of the charged MSPs in several ranges of mass. The payloads also carried Faraday rotation antennas and an array of plasma probes for determining electron and ion densities and the payload charging potential, thus providing a comprehensive picture of the distribution of charges over a wide range of altitudes that can be compared with models for the vertical distribution of MSPs and for the distribution of charge. The launches were from the Andoya Rocket Range, Norway, following the end of the noctilucent cloud season to avoid detection of ice. A night launch (11 October 21:50 UT) and a day launch (13 October 13:50 UT) helped to elucidate the role of solar ultraviolet in determining the charge state of the particles. The night data show a distinct change in the charge state of MSPs at the D-region ledge (similar to 78 km) below which the density of free electrons is greatly reduced. Above the ledge, negative MSPs are detected at up to 92 km, have number densities reaching similar to 200 cm(-3), and positive MSPs are absent. Below the ledge, positive and negative MSPs are about equally abundant, each with densities of similar to 2000 cm(-3) at 70 km and with slightly lower densities at 60 km. The MSPs are seen predominantly in mass bins spanning 500-2000 amu and 2000-8000 amu, with more massive particles (radii above similar to 1.2 nm assuming a smoke particle density of 2 g/cm(3)) having number densities below the detection threshold (10 cm(-3)) and less massive particles being indistinguishable from ions. The daytime launch data show positive MSPs present only below the ledge and their number density is reduced to below 300 cm(-3). The daytime data show negative MSPs both above and below the D-region ledge and their number density is also reduced, perhaps as a consequence of photodetachment. Modeling of the charge state of the MSPs shows that the total number density of MSPs, charged and uncharged, is approximately 20,000 cm(-3) below the ledge and the model reproduces the absence of positive MSPs above the ledge. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Robertson, Scott; Dickson, Shannon; Horanyi, Mihaly; Sternovsky, Zoltan] Univ Colorado, Boulder, CO 80304 USA.
   [Friedrich, Martin] Graz Univ Technol, A-8010 Graz, Austria.
   [Janches, Diego] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Megner, Linda] Stockholm Univ, Dept Meteorol, S-10691 Stockholm, Sweden.
   [Williams, Bifford] GATS Inc, Boulder, CO 80301 USA.
RP Dickson, S (reprint author), Univ Colorado, Ctr Integrated Plasma Studies, UCB 390, Boulder, CO 80309 USA.
EM Scott.Robertson@colorado.edu
RI Janches, Diego/D-4674-2012; 
OI Janches, Diego/0000-0001-8615-5166; STERNOVSKY,
   ZOLTAN/0000-0002-9658-1350; Horanyi, Mihaly/0000-0002-5920-9226
FU NASA Low Cost Access to Space program
FX The authors thank Michael Gausa, Scott Knappmiller, Rick Kohnert, Devin
   Konecny, Tyler Nickerson, and the staff of the Wallops Flight Facility.
   This research was support by the NASA Low Cost Access to Space program.
NR 82
TC 7
Z9 7
U1 0
U2 11
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 2014
VL 118
SI SI
BP 161
EP 179
DI 10.1016/j.jastp.2013.07.007
PN B
PG 19
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA AN1HI
UT WOS:000340332900005
ER

PT J
AU Dubovik, O
   Labonnote, L
   Litvinov, P
   Parol, F
   Mishchenko, MI
AF Dubovik, Oleg
   Labonnote, Laurent
   Litvinov, Pavel
   Parol, Frederic
   Mishchenko, Michael I.
TI Electromagnetic and Light Scattering by Nonspherical Particles XIV
   Preface
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Editorial Material
ID SPECIAL-ISSUE
C1 [Dubovik, Oleg] Univ Lille 1, Opt Atmospher Lab, CNRS, UMR8518, F-59655 Villeneuve Dascq, France.
   [Labonnote, Laurent; Litvinov, Pavel; Parol, Frederic] Univ Lille 1, Opt Atmospher Lab, UMR8518, F-59655 Villeneuve Dascq, France.
   [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 oleg.dubovik@univ-lille1.fr; Laurent.Labonnote@univ-lille1.fr;
   Pavel.Litvinov@univ-lille1.fr; frederic.parol@univ-lille1.fr;
   crmim2@gmail.com
RI Mishchenko, Michael/D-4426-2012
NR 13
TC 1
Z9 1
U1 2
U2 8
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 2014
VL 146
SI SI
BP 1
EP 3
DI 10.1016/j.jqsrt.2014.04.006
PG 3
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AM2RA
UT WOS:000339697300001
ER

PT J
AU Mishchenko, MI
AF Mishchenko, Michael I.
TI Directional radiometry and radiative transfer: The convoluted path from
   centuries-old phenomenology to physical optics
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Electromagnetic scattering; Physical optics; Directional radiometry;
   Radiative transfer; Macroscopic Maxwell equations; Mesoscopic physics
ID FREE ELECTROMAGNETIC-FIELDS; MULTIPLE-SCATTERING; SPHERICAL-PARTICLES;
   TRANSFER EQUATION; ABSORBING MEDIUM; QUANTUM-THEORY; COHERENT
   BACKSCATTERING; DISCRETE SCATTERERS; WEAK-LOCALIZATION; LIGHT-SCATTERING
AB This Essay traces the centuries-long history of the phenomenological disciplines of directional radiometry and radiative transfer in turbid media, discusses their fundamental weaknesses, and outlines the convoluted process of their conversion into legitimate branches of physical optics. Published by Elsevier Ltd.
C1 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 crmim2@gmail.com
RI Mishchenko, Michael/D-4426-2012
FU National Academy of Sciences of Ukraine; NASA Radiation Sciences
   Program; NASA Remote Sensing Theory Program
FX I appreciate numerous illuminating discussions with Anatoli Borovoi,
   Oleg Bugaenko, Brian Cairns, Helmut Domke, Joop Hovenier, Vsevolod
   Ivanov, Michael Kahnert, Nikolai Khlebtsov, Pavel Litvinov, Daniel
   Mackowski, M. Pinar Menguc, Viktor Tishkovets, Larry Travis, Cornelis
   van der Mee, Ping Yang, and Edgard Yanovitskij. Brian Cairns, Joop
   Hovenier, Michael Kahnert, Pavel Litvinov, Daniel Mackowski, M. Pinar
   Menguc, Larry Travis, and an anonymous referee provided encouraging and
   helpful comments on a preliminary version of this Essay, while Lilly Del
   Valle helped with graphics. My research has been partially funded over
   the years by the National Academy of Sciences of Ukraine, the NASA
   Radiation Sciences Program managed by Hal Maring, and the NASA Remote
   Sensing Theory Program managed by Lucia Tsaoussi.
NR 207
TC 11
Z9 11
U1 1
U2 16
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 2014
VL 146
SI SI
BP 4
EP 33
DI 10.1016/j.jqsrt.2014.02.033
PG 30
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AM2RA
UT WOS:000339697300002
ER

PT J
AU Bi, L
   Yang, P
   Liu, C
   Yi, BQ
   Baum, BA
   van Diedenhoven, B
   Iwabuchi, H
AF Bi, Lei
   Yang, Ping
   Liu, Chao
   Yi, Bingqi
   Baum, Bryan A.
   van Diedenhoven, Bastiaan
   Iwabuchi, Hironobu
TI Assessment of the accuracy of the conventional ray-tracing technique:
   Implications in remote sensing and radiative transfer involving ice
   clouds
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Ice clouds; Light scattering; Remote sensing; Radiative transfer
ID DIFFERENCE TIME-DOMAIN; DISCRETE-DIPOLE APPROXIMATION; SINGLE-SCATTERING
   PROPERTIES; LIGHT-SCATTERING; ELECTROMAGNETIC SCATTERING; CIRRUS CLOUDS;
   T-MATRIX; OPTICAL-THICKNESS; SOLAR-RADIATION; INHOMOGENEOUS PARTICLES
AB A fundamental problem in remote sensing and radiative transfer simulations involving ice clouds is the ability to compute accurate optical properties for individual ice particles. While relatively simple and intuitively appealing, the conventional geometric-optics method (CGOM) is used frequently for the solution of light scattering by ice crystals. Due to the approximations in the ray-tracing technique, the CGOM accuracy is not well quantified. The result is that the uncertainties are introduced that can impact many applications. Improvements in the Invariant Imbedding T-matrix method (II-TM) and the Improved Geometric-Optics Method (IGOM) provide a mechanism to assess the aforementioned uncertainties. The results computed by the II-TM + IGOM are considered as a benchmark because the II-TM solves Maxwell's equations from first principles and is applicable to particle size parameters ranging into the domain at which the IGOM has reasonable accuracy. To assess the uncertainties with the CGOM in remote sensing and radiative transfer simulations, two independent optical property datasets of hexagonal columns are developed for sensitivity studies by using the CGOM and the II-TM + IGOM, respectively. Ice cloud bulk optical properties obtained from the two datasets are compared and subsequently applied to retrieve the optical thickness and effective diameter from Moderate Resolution Imaging Spectroradiometer (MODIS) measurements. Additionally, the bulk optical properties are tested in broadband radiative transfer (RT) simulations using the general circulation model (GCM) version of the Rapid Radiative Transfer Model (RRTMG) that is adopted in the National Center for Atmospheric Research (NCAR) Community Atmosphere Model (CAM, version 5.1). For MODIS retrievals, the mean bias of uncertainties of applying the CGOM in shortwave bands (0.86 and 2.13 mu m) can be up to 5% in the optical thickness and as high as 20% in the effective diameter, depending on cloud optical thickness and effective diameter. In the MODIS infrared window bands centered at 8.5, 11, and 12 mu m, biases in the optical thickness and effective diameter are up to 12% and 10%, respectively. The CGOM-based simulation errors in ice cloud radiative forcing calculations are on the order of 10 W m(-2). (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Bi, Lei; Yang, Ping; Liu, Chao; Yi, Bingqi] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
   [Baum, Bryan A.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI 53706 USA.
   [van Diedenhoven, Bastiaan] Columbia Univ, NASA, Goddard Inst Space Studies, Ctr Climate Syst Res, New York, NY 10025 USA.
   [Iwabuchi, Hironobu] Tohoku Univ, Grad Sch Sci, Sendai, Miyagi 980, Japan.
RP Bi, L (reprint author), Texas A&M Univ, Dept Atmospher Sci, TAMU 3150, College Stn, TX 77843 USA.
EM bilei@tamu.edu
RI Yi, Bingqi/E-4076-2012; Baum, Bryan/B-7670-2011; Yang, Ping/B-4590-2011;
   Liu, Chao/J-9551-2013; Bi, Lei/B-9242-2011; 
OI Yi, Bingqi/0000-0002-1437-8376; Baum, Bryan/0000-0002-7193-2767;
   Iwabuchi, Hironobu/0000-0002-9311-8598; van Diedenhoven,
   Bastiaan/0000-0001-5622-8619
FU National Science Foundation (NSF) [AGS-1338440]; NASA [NNX11A1K37G,
   NNX11AF40G]; University of Wisconsin-Madison [301K630]
FX This study was supported by a National Science Foundation (NSF) Grant
   (AGS-1338440), NASA Grants (NNX11A1K37G and NNX11AF40G), and a
   subcontract (301K630) to Texas A&M University from the University of
   Wisconsin-Madison. A major portion of the simulations was carried out at
   the Texas A&M University Supercomputing Facilities, and the authors
   gratefully acknowledge Facility staff for their help and assistance. The
   authors also gratefully acknowledge the effort by the anonymous
   reviewers to improve this manuscript
NR 68
TC 13
Z9 14
U1 0
U2 13
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 2014
VL 146
SI SI
BP 158
EP 174
DI 10.1016/j.jqsrt.2014.03.017
PG 17
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AM2RA
UT WOS:000339697300012
ER

PT J
AU Dlugach, JM
   Mishchenko, MI
AF Dlugach, Janna M.
   Mishchenko, Michael I.
TI Effects of nonsphericity on the behavior of Lorenz-Mie resonances in
   scattering characteristics of liquid-cloud droplets
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Lorenz-Mie resonances; Averaging over sizes; Averaging over
   orientations; Scattering characteristics; Nonspherical particles; Cloud
   droplets; T-matrix method
ID EXTINCTION CROSS-SECTION; DIELECTRIC SPHERES
AB By using the results of highly accurate T-matrix computations for randomly oriented oblate and prolate spheroids and Chebyshev particles with varying degrees of asphericity, we analyze the effects of a deviation of water-droplet shapes from that of a perfect sphere on the behavior of Lorenz-Mie morphology-dependent resonances of various widths. We demonstrate that the positions and profiles of the resonances can change significantly with increasing asphericity. The absolute degree of asphericity required to suppress a Lorenz-Mie resonance is approximately proportional to the resonance width. Our results imply that numerical averaging of scattering characteristics of real cloud droplets over sizes may rely on a significantly coarser size-parameter resolution than that required for ideal, perfectly spherical particles. 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 crmim2@gmail.com
RI Mishchenko, Michael/D-4426-2012
FU NASA Radiation Sciences Program; NASA Remote Sensing Theory Program;
   National Academy of Sciences of Ukraine under the Main Astronomical
   Observatory GRAPE/GPU/GRID Computing Cluster Project
FX We thank S. Hill for providing his computer program for the calculation
   of Lorenz-Mie MDR locations and widths. This research was partly funded
   by the NASA Radiation Sciences Program managed by Hal Maring and by the
   NASA Remote Sensing Theory Program managed by Lucia Tsaoussi. We also
   acknowledge support from the National Academy of Sciences of Ukraine
   under the Main Astronomical Observatory GRAPE/GPU/GRID Computing Cluster
   Project.
NR 17
TC 1
Z9 1
U1 0
U2 12
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 2014
VL 146
SI SI
BP 227
EP 234
DI 10.1016/j.jqsrt.2014.01.004
PG 8
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AM2RA
UT WOS:000339697300019
ER

PT J
AU Mishchenko, MI
   Zakharova, NT
   Khlebtsov, NG
   Wriedt, T
   Videen, G
AF Mishchenko, Michael I.
   Zakharova, Nadezhda T.
   Khlebtsov, Nikolai G.
   Wriedt, Thomas
   Videen, Gorden
TI Comprehensive thematic T-matrix reference database: A 2013-2014 update
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Electromagnetic scattering; T-matrix method; Complex scattering objects
ID DEPOLARIZED LIGHT-SCATTERING; POLAR STRATOSPHERIC CLOUDS; PARTICLE
   NON-SPHERICITY; X-BAND RADAR; OPTICAL-PROPERTIES; SINGLE-SCATTERING;
   MICROWAVE LINKS; ELECTROMAGNETIC SCATTERING; COHERENT BACKSCATTERING;
   HETEROGENEOUS FORMATION
AB This paper is the sixth update to the comprehensive thematic database of peer-reviewed T-matrix publications initiated by us in 2004 and includes relevant publications that have appeared since 2013. It also lists several earlier publications not incorporated in the original database and previous updates. Published by Elsevier Ltd.
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
   [Zakharova, Nadezhda T.] Trinnovim LLC, New York, NY 10025 USA.
   [Khlebtsov, Nikolai G.] Russian Acad Sci, Inst Biochem & Physiol Plants & Microorganisms, Saratov 410015, Russia.
   [Wriedt, Thomas] Inst Werkstofftech, D-28359 Bremen, Germany.
   [Videen, Gorden] US Army, Res Lab, AMSRL IS EE, Adelphi, MD 20783 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM crmim2@gmail.com
RI Mishchenko, Michael/D-4426-2012; Khlebtsov, Nikolai/D-6199-2017; 
OI Khlebtsov, Nikolai/0000-0002-2055-7784
FU NASA Radiation Sciences Program; NASA Remote Sensing Theory Program;
   RFBR; Russian Scientific Foundation
FX We thank Josefina Mora and Zoe Wai for helping to obtain copies of
   publications that were not readily accessible. MIM was supported by the
   NASA Radiation Sciences Program managed by Hal Maring and by the NASA
   Remote Sensing Theory Program managed by Lucia Tsaoussi. NGK was
   supported by grants from RFBR and Russian Scientific Foundation.
NR 158
TC 22
Z9 23
U1 2
U2 38
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 2014
VL 146
SI SI
BP 349
EP 354
DI 10.1016/j.jqsrt.2014.03.022
PG 6
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AM2RA
UT WOS:000339697300031
ER

PT J
AU van Diedenhoven, B
AF van Diedenhoven, Bastiaan
TI The prevalence of the 22 degrees halo in cirrus clouds
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Ice crystals; Cirrus clouds; Halos
ID HEXAGONAL ICE CRYSTALS; MULTIDIRECTIONAL POLARIZATION MEASUREMENTS;
   SINGLE-SCATTERING PROPERTIES; RADIATIVE PROPERTIES; OPTICAL-PROPERTIES;
   LIGHT-SCATTERING; REFLECTANCES; AIRCRAFT; MODELS
AB Halos at 22 degrees from the sun attributed to randomly-orientated, pristine hexagonal crystals are frequently observed through ice clouds. These frequent sightings of halos formed by pristine crystals pose an apparent inconsistency with the dominance of distorted, non-pristine ice crystals indicated by in situ and remote sensing data. Furthermore, the 46 degrees halo, which is associated with pristine hexagonal crystals as well, is observed far less frequently than the 22 degrees halo. Considering that plausible mechanisms that could cause crystal distortion such as aggregation, sublimation, riming and collisions are stochastic processes that likely lead to distributions of crystals with varying distortion levels, here the presence of the 22 degrees and 46 degrees halo features in phase functions of mixtures of pristine and distorted hexagonal ice crystals is examined. We conclude that the 22 degrees halo feature is generally present if the contribution by pristine crystals to the total scattering cross section is greater than only about 10% in the case of compact particles or columns, and greater than about 40% for plates. The 46 degrees halo feature is present only if the mean distortion level is low and the contribution of pristine crystals to the total scattering cross section is above about 20%, 50% and 70%, in the case of compact crystals, plates and columns, respectively. These results indicate that frequent sightings of 22 degrees halos are not inconsistent with the observed dominance of distorted, non-pristine ice crystals. Furthermore, the low mean distortion levels and large contributions by pristine crystals needed to produce the 46 degrees halo features provide a potential explanation of the common sighting of the 22 degrees halo without any detectable 46 degrees halo. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [van Diedenhoven, Bastiaan] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
   [van Diedenhoven, Bastiaan] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP van Diedenhoven, B (reprint author), Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA.
EM bastiaan.vandiedenhoven@nasa.gov
OI van Diedenhoven, Bastiaan/0000-0001-5622-8619
NR 36
TC 6
Z9 6
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 2014
VL 146
SI SI
BP 475
EP 479
DI 10.1016/j.jqsrt.2014.01.012
PG 5
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AM2RA
UT WOS:000339697300045
ER

PT J
AU Wang, J
   Xu, XG
   Ding, SG
   Zeng, J
   Spurr, R
   Liu, X
   Chance, K
   Mishchenko, M
AF Wang, Jun
   Xu, Xiaoguang
   Ding, Shouguo
   Zeng, Jing
   Spurr, Robert
   Liu, Xiong
   Chance, Kelly
   Mishchenko, Michael
TI A numerical testbed for remote sensing of aerosols, and its
   demonstration for evaluating retrieval synergy from a geostationary
   satellite constellation of GEO-CAPE and GOES-R
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Testbed of remote sensing of aerosols; GEO-CAPE; TEMPO; GOES-R;
   Optimization; Linearized codes for radiative transfer and scattering
ID ABSORPTION CROSS-SECTIONS; OZONE UV SPECTROSCOPY; RADIATIVE-TRANSFER;
   NEXT-GENERATION; MISSION; ALGORITHM; CAPABILITIES; TEMPERATURE;
   SENSITIVITY; MODELS
AB We present a numerical testbed for remote sensing of aerosols, together with a demonstration for evaluating retrieval synergy from a geostationary satellite constellation. The testbed combines inverse (optimal-estimation) software with a forward model containing linearized code for computing particle scattering (for both spherical and non-spherical particles), a kernel-based (land and ocean) surface bi-directional reflectance facility, and a linearized radiative transfer model for polarized radiance. Calculation of gas absorption spectra uses the HITRAN (High-resolution TRANsmission molecular absorption) database of spectroscopic line parameters and other trace species cross-sections. The outputs of the testbed include not only the Stokes 4-vector elements and their sensitivities (Jacobians) with respect to the aerosol single scattering and physical parameters (such as size and shape parameters, refractive index, and plume height), but also DFS (Degree of Freedom for Signal) values for retrieval of these parameters. This testbed can be used as a tool to provide an objective assessment of aerosol information content that can be retrieved for any constellation of (planned or real) satellite sensors and for any combination of algorithm design factors (in terms of wavelengths, viewing angles, radiance and/or polarization to be measured or used). We summarize the components of the testbed, including the derivation and validation of analytical formulae for Jacobian calculations. Benchmark calculations from the forward model are documented. In the context of NASA's Decadal Survey Mission GEO-CAPE (GEOstationary Coastal and Air Pollution Events), we demonstrate the use of the testbed to conduct a feasibility study of using polarization measurements in and around the O-2 A band for the retrieval of aerosol height information from space, as well as an to assess potential improvement in the retrieval of aerosol fine and coarse mode aerosol optical depth (AOD) through the synergic use of two future geostationary satellites, GOES-R (Geostationary Operational Environmental Satellite R-series) and TEMPO (Tropospheric Emissions: Monitoring of Pollution). Strong synergy between GEOS-R and TEMPO are found especially in their characterization of surface bi-directional reflectance, and thereby, can potentially improve the AOD retrieval to the accuracy required by GEO-CAPE. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Wang, Jun; Xu, Xiaoguang; Ding, Shouguo; Zeng, Jing] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA.
   [Spurr, Robert] RT Solut Inc, Cambridge, MA 02138 USA.
   [Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Mishchenko, Michael] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Wang, J (reprint author), Univ Nebraska, Dept Earth & Atmospher Sci, 303 Bessey Hall, Lincoln, NE 68588 USA.
EM jwang7@unl.edu
RI Mishchenko, Michael/D-4426-2012; Liu, Xiong/P-7186-2014; Xu,
   Xiaoguang/B-8203-2016; Wang, Jun/A-2977-2008; 
OI Liu, Xiong/0000-0003-2939-574X; Xu, Xiaoguang/0000-0001-9583-980X; Wang,
   Jun/0000-0002-7334-0490; Chance, Kelly/0000-0002-7339-7577
FU NASA Earth Science Division, GEO-CAPE mission study and Glory mission
   science activities
FX Funding for this study was provided by the NASA Earth Science Division
   as part of GEO-CAPE mission study and Glory mission science activities.
   J. Wang is grateful to Jassim (Jay) A. Al-Saadi and Hal H. Maring for
   their support, and thanks the GEO-CAPE aerosol working group and science
   working group for their constructive suggestions and fruitful
   discussions. The Holland Computing Center of University of Nebraska -
   Lincoln and NASA High End Computing program are acknowledged for their
   help in computing.
NR 65
TC 12
Z9 13
U1 1
U2 29
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 2014
VL 146
SI SI
BP 510
EP 528
DI 10.1016/j.jqsrt.2014.03.020
PG 19
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA AM2RA
UT WOS:000339697300049
ER

PT J
AU Driggers, WB
   Frazier, BS
   Adams, DH
   Ulrich, GF
   Jones, CM
   Hoffmayer, ER
   Campbell, MD
AF Driggers, William B., III
   Frazier, Bryan S.
   Adams, Douglas H.
   Ulrich, Glenn F.
   Jones, Christian M.
   Hoffmayer, Eric R.
   Campbell, Matthew D.
TI Site fidelity of migratory bonnethead sharks Sphyrna tiburo (L. 1758) to
   specific estuaries in South Carolina, USA
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Bonnethead; Habitat utilization; Movement patterns; Residency; Site
   fidelity
ID ATLANTIC SHARPNOSE SHARK; GULF-OF-MEXICO; HABITAT USE;
   CARCHARODON-CARCHARIAS; GALEOCERDO-CUVIER; HAMMERHEAD SHARK;
   FEEDING-HABITS; UNITED-STATES; LIFE-HISTORY; WHITE SHARKS
AB To examine the migratory patterns, habitat utilization and residency of bonnethead sharks (Sphyrna tiburo (L 1758)) in estuarine systems within coastal South Carolina, a tag-recapture experiment was conducted from 1998 to 2012 during which 2300 individuals were tagged. To assess the intra and inter-annual movements of tagged sharks, six estuaries within state waters were monitored using multiple gear types in addition to the cooperative efforts of recreational anglers throughout the southeastern United States. Over the course of the experiment 177 bonnetheads were recaptured after 3 days to 8.9 years at liberty, representing a recapture rate of approximately 8%. All bonnetheads were recaptured within the same estuary where they were originally tagged on intra and/or inter-annual scales, with the exception of six individuals, which were recaptured during migratory periods (i.e. late fall, winter and spring) in coastal waters off Florida, Georgia, North Carolina, and South Carolina. On 23 occasions cohesion was demonstrated by groups ranging in size from 2 to 5 individuals that were tagged together and recaptured together, with times at liberty ranging from 12 days to 3.6 years. Additionally, 13 individuals were recaptured multiple times with times at liberty ranging from 12 days to 8.9 years; all individuals were recaptured in the same estuary where they were initially tagged. We hypothesize that bonnetheads are using South Carolina's estuaries as summer feeding grounds due to the relatively high abundance of blue crabs (Callinectes sapidus), including ovigerous females during spring and summer months, and the location of these ephemeral yet predictable feeding areas is socially transmitted to relatively young, naive sharks by experienced, older individuals. The high degree of intra and inter-annual site fidelity demonstrated by bonnetheads in this region offers unique opportunities for in situ study of various aspects of the biology of this species, including identification of essential habitats, growth, homing mechanisms, mortality rates, movement patterns and social behavior. Published by Elsevier B.V.
C1 [Driggers, William B., III; Jones, Christian M.; Hoffmayer, Eric R.; Campbell, Matthew D.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA.
   [Frazier, Bryan S.; Ulrich, Glenn F.] South Carolina Dept Nat Resources, Charleston, SC 29412 USA.
   [Adams, Douglas H.] Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, Melbourne, FL 32901 USA.
RP Driggers, WB (reprint author), Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA.
EM william.driggers@noaa.gov
OI Campbell, Matthew/0000-0002-0087-5291
FU Cooperative Atlantic States Shark Pupping and Nursery Habitat Survey;
   South Carolina State Recreational Fisheries Advisory Committee
FX We thank Karl Brenkert, Henry Davega, Carrie Hendrix, Doug Mellichamp,
   Doug Oakley, Catherine Riley, Ashley Shaw and Paul Tucker for their
   assistance during the field portion of this study and the Inshore
   Fisheries Division of SCDNR for use of the trammel net data. We also
   thank Cami McCandless, Pat Turner, Nancy Kohler and Ruth Briggs with the
   NMFS Apex Program for providing tags. Aspects of this work were funded
   in part by the Cooperative Atlantic States Shark Pupping and Nursery
   Habitat Survey and the South Carolina State Recreational Fisheries
   Advisory Committee.
NR 50
TC 8
Z9 8
U1 8
U2 39
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 2014
VL 459
BP 61
EP 69
DI 10.1016/j.jembe.2014.05.006
PG 9
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA AL4TU
UT WOS:000339128500009
ER

PT J
AU Liewer, PC
   Hernandez, IG
   Hall, JR
   Lindsey, C
   Lin, X
AF Liewer, P. C.
   Hernandez, I. Gonzalez
   Hall, J. R.
   Lindsey, C.
   Lin, X.
TI Testing the Reliability of Predictions of Far-Side Active Regions from
   Helioseismology Using STEREO Far-Side Observations of Solar Activity
SO SOLAR PHYSICS
LA English
DT Article
DE Active regions; Corona; Helioseismology; Space weather
ID SUN
AB We test the reliability of helioseismic far-side active-region predictions, made using Dopplergrams from both the Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO) and the Global Oscillation Network Group (GONG), by comparison with far-side observation of solar activity from the Solar TErrestrial RElations Observatory (STEREO). Both GONG and HMI produce seismic Carrington maps that show strong magnetic-field regions, labeling predictions of far-side active regions that have a probability >= 70 %. By visual comparison of these prediction maps with STEREO extreme ultraviolet (EUV) Carrington maps, we determine whether or not solar activity, as evidenced as brightness in EUV, is observed at the predicted locations. We analyzed nine months of data from 2011 and 2012. For both GONG and HMI, we find that for approximately 90 % of the active-region predictions, activity/brightness is observed in EUV at the predicted location. We also investigated the success of GONG and HMI at predicting large active regions before they appear at the east limb as viewed from Earth. Of the 27 identified large east-limb active regions in the nine months of data analyzed, GONG predicted 15 (55 %) at least once within the week prior to Earth-side appearance and HMI predicted 13 (48 %). Based on the STEREO far-side EUV observations, we suggest that 9 of the 27 active regions were probably too weak to be predicted while on the far side. Overall, we conclude that HMI and GONG have similar reliability using the current data-processing procedures.
C1 [Liewer, P. C.; Hall, J. R.; Lin, X.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Hernandez, I. Gonzalez] Natl Solar Observ, Tucson, AZ 85719 USA.
   [Lindsey, C.] Northwest Res Associates, Boulder, CO 80301 USA.
RP Liewer, PC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Paulett.Liewer@jpl.nasa.gov
FU NASA [NNH10CD50C]
FX We would like to thank P. Scherrer and A. Kosovichev for informative
   discussions on the use of helioseismology to make far-side active-region
   predictions. We would like to thank W.T. Thompson for his invaluable
   help with processing the EUV data. We also thank E. De Jong, M. Velli
   and A. Vourlidas for useful discussions of this research. Finally, we
   would like to thank the reviewer for valuable comments. The work of PCL,
   JRH and XL was conducted at the Jet Propulsion Laboratory, California
   Institute of Technology under a contract from NASA. The work of IGH was
   supported by the NASA Living with a Star Targeted Research and
   Technology Program. The work of CL was supported by NASA Contract
   NNH10CD50C. The STEREO/SECCHI data used here are produced by an
   international consortium of the Naval Research Laboratory (USA),
   Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard Space
   Flight Center (USA) Rutherford Appleton Laboratory (UK), University of
   Birmingham (UK), Max-Planck-Institut fur Sonnensystemforschung
   (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique
   Theorique et Applique (France), Institut d'Astrophysique Spatiale
   (France). This work utilizes data obtained by the Global Oscillation
   Network Group (GONG) Program. GONG is managed by the National Solar
   Observatory, which is operated by AURA, Inc. under a cooperative
   agreement with the NSF. The GONG data were acquired by instruments
   operated by the Big Bear Solar Observatory, High Altitude Observatory,
   Learmonth Solar Observatory, Udaipur Solar Observatory, Instituto de
   Astrofisica de Canarias, and Cerro Tololo Interamerican Observatory. The
   HMI data were provided by NASA through the Joint Science Operations
   Center for the SDO project at Stanford University.
NR 18
TC 3
Z9 3
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 OCT
PY 2014
VL 289
IS 10
BP 3617
EP 3640
DI 10.1007/s11207-014-0542-6
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8JQ
UT WOS:000339384900002
ER

PT J
AU Wang, TJ
   Davila, JM
AF Wang, Tongjiang
   Davila, Joseph M.
TI Validation of Spherically Symmetric Inversion by Use of a
   Tomographically Reconstructed Three-Dimensional Electron Density of the
   Solar Corona
SO SOLAR PHYSICS
LA English
DT Article
DE Sun: corona; Methods: data analysis; STEREO; COR1
ID WHOLE SUN MONTH; WHITE-LIGHT IMAGES; MASS EJECTIONS; MAGNETOHYDRODYNAMIC
   SIMULATIONS; PARTICLE-ACCELERATION; SCALE STRUCTURES; MAGNETIC-FIELD;
   STREAMER BELT; MHD MODELS; F-CORONA
AB Determining the coronal electron density by the inversion of white-light polarized brightness (pB) measurements by coronagraphs is a classic problem in solar physics. An inversion technique based on the spherically symmetric geometry (spherically symmetric inversion, SSI) was developed in the 1950s and has been widely applied to interpret various observations. However, to date there is no study of the uncertainty estimation of this method. We here present the detailed assessment of this method using a three-dimensional (3D) electron density in the corona from 1.5 to 4 R (aS (TM)) as a model, which is reconstructed by a tomography method from STEREO/COR1 observations during the solar minimum in February 2008 (Carrington Rotation, CR 2066). We first show in theory and observation that the spherically symmetric polynomial approximation (SSPA) method and the Van de Hulst inversion technique are equivalent. Then we assess the SSPA method using synthesized pB images from the 3D density model, and find that the SSPA density values are close to the model inputs for the streamer core near the plane of the sky (POS) with differences generally smaller than about a factor of two; the former has the lower peak but extends more in both longitudinal and latitudinal directions than the latter. We estimate that the SSPA method may resolve the coronal density structure near the POS with angular resolution in longitude of about 50A degrees. Our results confirm the suggestion that the SSI method is applicable to the solar minimum streamer (belt), as stated in some previous studies. In addition, we demonstrate that the SSPA method can be used to reconstruct the 3D coronal density, roughly in agreement with the reconstruction by tomography for a period of low solar activity (CR 2066). We suggest that the SSI method is complementary to the 3D tomographic technique in some cases, given that the development of the latter is still an ongoing research effort.
C1 [Wang, Tongjiang] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
   [Wang, Tongjiang; Davila, Joseph M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Wang, TJ (reprint author), Catholic Univ Amer, Dept Phys, 620 Michigan Ave NE, Washington, DC 20064 USA.
EM tongjiang.wang@nasa.gov
FU NASA [NNG11PL10A, NNX12AB34G]
FX The work of TW was supported by the NASA Cooperative Agreement
   NNG11PL10A to the Catholic University of America and NASA grant
   NNX12AB34G. We very much appreciate the suggestions of Maxim Kramar,
   which led to an improved estimate of the angular resolution of the SSPA
   method in Appendix. We also thank the anonymous referee for his/her
   valuable comments that improved the manuscript.
NR 64
TC 5
Z9 5
U1 4
U2 13
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 OCT
PY 2014
VL 289
IS 10
BP 3723
EP 3745
DI 10.1007/s11207-014-0556-0
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8JQ
UT WOS:000339384900007
ER

PT J
AU Richardson, IG
AF Richardson, I. G.
TI Identification of Interplanetary Coronal Mass Ejections at Ulysses Using
   Multiple Solar Wind Signatures
SO SOLAR PHYSICS
LA English
DT Article
DE Coronal mass ejections; Interplanetary coronal mass ejections;
   Interplanetary magnetic field; Magnetic clouds; Solar wind plasma;
   Ulysses
ID IN-SITU OBSERVATIONS; ION CHARGE-STATE; PROTON TEMPERATURE; OUTER
   HELIOSPHERE; IONIZATION STATE; MAGNETIC CLOUDS; CYCLE 23; ENERGETIC
   PARTICLES; HELIUM ABUNDANCE; SOURCE LOCATION
AB Previous studies have discussed the identification of interplanetary coronal mass ejections (ICMEs) near the Earth based on various solar wind signatures. In particular, methods have been developed of identifying regions of anomalously low solar wind proton temperatures (T (p)) and plasma compositional anomalies relative to the composition of the ambient solar wind that are frequently indicative of ICMEs. In this study, similar methods are applied to observations from the Ulysses spacecraft that was launched in 1990 and placed in a heliocentric orbit over the poles of the Sun. Some 279 probable ICMEs are identified during the spacecraft mission, which ended in 2009. The identifications complement those found independently in other studies of the Ulysses data, but a number of additional events are identified. The properties of the ICMEs detected at Ulysses and those observed near the Earth and in the inner heliosphere are compared.
C1 [Richardson, I. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Richardson, I. G.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
   [Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Richardson, IG (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
EM ian.g.richardson@nasa.gov
OI Richardson, Ian/0000-0002-3855-3634
FU NASA
FX We are indebted to the many Ulysses experimenters who provided the
   observations used in this study, which were obtained from the Space
   Physics Data Facility at GSFC (http://spdf.gsfc.nasa.gov/). Data in
   Figure 15 from the LASCO coronagraphs on SOHO were obtained from the
   GSFC/Catholic University of America catalog
   http://cdaw.gsfc.nasa.gov/CME_list/; SOHO is a project of international
   cooperation between ESA and NASA. ACE observations were obtained from
   the ACE Science Center (http://www.srl.caltech.edu/ACE/ASC/). This work
   was supported by a NASA Guest Investigator Award.
NR 90
TC 2
Z9 2
U1 1
U2 5
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 OCT
PY 2014
VL 289
IS 10
BP 3843
EP 3894
DI 10.1007/s11207-014-0540-8
PG 52
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8JQ
UT WOS:000339384900012
ER

PT J
AU Belov, A
   Abunin, A
   Abunina, M
   Eroshenko, E
   Oleneva, V
   Yanke, V
   Papaioannou, A
   Mavromichalaki, H
   Gopalswamy, N
   Yashiro, S
AF Belov, A.
   Abunin, A.
   Abunina, M.
   Eroshenko, E.
   Oleneva, V.
   Yanke, V.
   Papaioannou, A.
   Mavromichalaki, H.
   Gopalswamy, N.
   Yashiro, S.
TI Coronal Mass Ejections and Non-recurrent Forbush Decreases
SO SOLAR PHYSICS
LA English
DT Article
DE Forbush decreases; Coronal mass ejections; Solar wind; Interplanetary
   coronal mass ejections; Neutron monitors
ID COSMIC-RAY MODULATION; SOLAR-WIND DISTURBANCES; MISSION; STEREO; FLARES
AB Coronal mass ejections (CMEs) and their interplanetary counterparts (interplanetary coronal mass ejections, ICMEs) are responsible for large solar energetic particle events and severe geomagnetic storms. They can modulate the intensity of Galactic cosmic rays, resulting in non-recurrent Forbush decreases (FDs). We investigate the connection between CME manifestations and FDs. We used specially processed data from the worldwide neutron monitor network to pinpoint the characteristics of the recorded FDs together with CME-related data from the detailed online catalog based upon the Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronagraph (LASCO) data. We report on the correlations of the FD magnitude to the CME initial speed, the ICME transit speed, and the maximum solar wind speed. Comparisons between the features of CMEs (mass, width, velocity) and the characteristics of FDs are also discussed. FD features for halo, partial halo, and non-halo CMEs are presented and discussed.
C1 [Belov, A.; Abunin, A.; Abunina, M.; Eroshenko, E.; Oleneva, V.; Yanke, V.] Russian Acad Sci, IZMIRAN, Moscow, Russia.
   [Papaioannou, A.; Mavromichalaki, H.] Univ Athens, Dept Phys, Nucl & Particle Phys Sect, Athens 11528, Greece.
   [Papaioannou, A.] Natl Observ Athens, IAASARS, Athens, Greece.
   [Gopalswamy, N.] NASA, GSFC, Heliophys Div, Greenbelt, MD 20771 USA.
   [Yashiro, S.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Papaioannou, A (reprint author), Univ Athens, Dept Phys, Nucl & Particle Phys Sect, Athens 11528, Greece.
EM abelov@izmiran.ru; erosh@izmiran.ru; atpapaio@phys.uoa.gr;
   emavromi@phys.uoa.gr; Nat.Gopalswamy@nasa.gov
RI Papaioannou, Athanasios/K-7065-2013
FU NASA's LWS TR T program
FX The SOHO/LASCO/CME catalog is generated and maintained at the CDAW Data
   Center by NASA and The Catholic University of America in cooperation
   with the Naval Research Laboratory. SOHO is a project of international
   cooperation between ESA and NASA. The work of coauthors N. Gopalswamy
   and S. Yashiro is supported by NASA's LWS TR & T program. The authors
   would like to thank the anonymous referee for the careful evaluation of
   the manuscript.
NR 43
TC 10
Z9 11
U1 0
U2 5
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 OCT
PY 2014
VL 289
IS 10
BP 3949
EP 3960
DI 10.1007/s11207-014-0534-6
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AL8JQ
UT WOS:000339384900016
ER

PT J
AU Hulson, PJF
   Hanselman, DH
AF Hulson, Peter-John F.
   Hanselman, Dana H.
TI Tradeoffs between bias, robustness, and common sense when choosing
   selectivity forms
SO FISHERIES RESEARCH
LA English
DT Article
DE Age-structured assessment; Fishery and survey selectivity; Life history
ID STOCK ASSESSMENT; AGE; FISHERY; MODEL
AB Selectivity, as a combination of gear vulnerability and fish availability, can be modeled in age-structured assessment models with simple functions that range from those that employ a small number of parameters to those that use complex and highly parameterized functions. We conducted simulations across two life history types to test whether allowing more complicated selectivity forms is both estimable and justified when compared to simpler selectivity curves with a lower number of parameters. Operating models were constructed with asymptotic and dome-shaped fishery and survey selectivity and estimation models were evaluated that used a range of complexity in fishery selectivity from the 2-parameter logistic to the highly parameterized double normal function. Results indicated that in general, uncertainty and bias in final year spawning biomass was not consistent across the life history types, the parameterizations employed, or fishing to the left or right side of the maturity curve. For instance, estimating a dome shaped selectivity for the survey when the true selectivity was asymptotic did not result in positive bias in all cases, and, estimating asymptotic fishing selectivity was not always conservative. Overall, we find that more complex selectivity functions and even time-dependent parameterizations of selectivity may be robust for short-lived species, but may not be robust when applied to long-lived species. Published by Elsevier B.V.
C1 [Hulson, Peter-John F.; Hanselman, Dana H.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA.
RP Hulson, PJF (reprint author), NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM pete.hulson@noaa.gov
NR 22
TC 4
Z9 4
U1 0
U2 3
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 2014
VL 158
SI SI
BP 63
EP 73
DI 10.1016/j.fishres.2013.12.016
PG 11
WC Fisheries
SC Fisheries
GA AK7OO
UT WOS:000338617800007
ER

PT J
AU Pasareanu, CS
   Salaun, G
AF Pasareanu, Corina S.
   Salauen, Gwen
TI Special Issue on Formal Aspects of Component Software (Selected Papers
   from FACS'12) Preface
SO SCIENCE OF COMPUTER PROGRAMMING
LA English
DT Editorial Material
C1 [Pasareanu, Corina S.] NASA Ames, Moffett Field, CA 94035 USA.
   [Salauen, Gwen] Inria, Grenoble INP, Grenoble, France.
RP Pasareanu, CS (reprint author), NASA Ames, Moffett Field, CA 94035 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-6423
EI 1872-7964
J9 SCI COMPUT PROGRAM
JI Sci. Comput. Program.
PD OCT 1
PY 2014
VL 91
SI SI
BP 1
EP 2
DI 10.1016/j.scico.2014.01.015
PN A
PG 2
WC Computer Science, Software Engineering
SC Computer Science
GA AK4NL
UT WOS:000338401300001
ER

PT J
AU Lavalle, M
   Khun, K
AF Lavalle, Marco
   Khun, Kosal
TI Three-Baseline InSAR Estimation of Forest Height
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Interferometry; synthetic aperture radar
ID POLARIMETRIC SAR INTERFEROMETRY; TEMPORAL DECORRELATION; L-BAND;
   INVERSION; RADAR; QUANTIFICATION; MODEL
AB In this letter we propose a three-baseline approach to the extraction of forest tree height from synthetic aperture radar data. Three polarimetric-interferometric pairs are used to constrain a physical model that relates forest parameters to multiple repeat-pass coherence observations. The observations may be performed by a dual, compact or full polarimetric radar, and may be affected by distinct levels of temporal decorrelation. Here, we present the theoretical framework based on the random-motion-over-ground model, and describe an algorithm to extract tree height from the data. The performance of the algorithm is illustrated with L-band airborne data collected by the German Aerospace Center in the frame of the BIOSAR2008 campaign. The proposed method provides height estimates in good agreement with lidar measurements and can be applied to data to be collected by forthcoming polarimetric-interferometric spaceborne missions.
C1 [Lavalle, Marco] CALTECH, Jet Prop Lab, Radar Sci & Engn Sect, Pasadena, CA 91109 USA.
   [Khun, Kosal] Univ Montreal, Dept Geog, Montreal, PQ H3C 3J7, Canada.
RP Lavalle, M (reprint author), CALTECH, Jet Prop Lab, Radar Sci & Engn Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 20
TC 5
Z9 6
U1 1
U2 33
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 2014
VL 11
IS 10
BP 1737
EP 1741
DI 10.1109/LGRS.2014.2307583
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 AI8NH
UT WOS:000337174100015
ER

PT J
AU Le Vine, DM
   de Matthaeis, P
AF Le Vine, D. M.
   de Matthaeis, P.
TI Aquarius Active/Passive RFI Environment at L-Band
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE L-band; radio frequency interference; scatterometer
ID SALINITY
AB Active/Passive instrument combinations (i.e., radiometer and radar) are being developed at L-band for remote sensing of sea surface salinity and soil moisture. Aquarius is already in orbit and SMAP is planned for launch in the Fall of 2014. Aquarius has provided for the first time a simultaneous look at the Radio Frequency Interference (RFI) environment from space for both active and passive instruments. The RFI environment for the radiometer observations is now reasonably well known and examples from Aquarius are presented in this manuscript that show that RFI is an important consideration for the scatterometer as well. In particular, extensive areas of the USA, Europe and Asia exhibit strong RFI in both the radiometer band at 1.41 GHz and in the band at 1.26 GHz employed by the Aquarius scatterometer. Furthermore, in areas such as the USA, where RFI at 1.4 GHz is relatively well controlled, RFI in the scatterometer band maybe the limiting consideration for the operation of combination active/passive instruments.
C1 [Le Vine, D. M.; de Matthaeis, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Le Vine, DM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 10
TC 3
Z9 3
U1 2
U2 14
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 2014
VL 11
IS 10
BP 1747
EP 1751
DI 10.1109/LGRS.2014.2307794
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 AI8NH
UT WOS:000337174100017
ER

PT J
AU Proud, SR
   Zhang, QL
   Schaaf, C
   Fensholt, R
   Rasmussen, MO
   Shisanya, C
   Mutero, W
   Mbow, C
   Anyamba, A
   Pak, E
   Sandholt, I
AF Proud, Simon Richard
   Zhang, Qingling
   Schaaf, Crystal
   Fensholt, Rasmus
   Rasmussen, Mads Olander
   Shisanya, Chris
   Mutero, Wycliffe
   Mbow, Cheikh
   Anyamba, Assaf
   Pak, Ed
   Sandholt, Inge
TI The Normalization of Surface Anisotropy Effects Present in SEVIRI
   Reflectances by Using the MODIS BRDF Method
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Angular effects; anisotropy; bidirectional reflectance distribution
   function (BRDF); land surface reflectance; MODerate resolution Imaging
   Spectroradiometer (MODIS); Meteosat Second Generation (MSG) Spinning
   Enhanced Visible and InfraRed Imager (SEVIRI)
ID IN-SITU MEASUREMENTS; BIDIRECTIONAL REFLECTANCE; ALBEDO RETRIEVAL;
   SEMIARID ENVIRONMENT; VEGETATION INDEXES; ATMOSPHERIC CORRECTION; EARTHS
   SURFACE; LAND; METEOSAT; MODEL
AB A modified version of the MODerate resolution Imaging Spectroradiometer (MODIS) bidirectional reflectance distribution function (BRDF) algorithm is presented for use in the angular normalization of surface reflectance data gathered by the Spinning Enhanced Visible and InfraRed Imager (SEVIRI) aboard the geostationary Meteosat Second Generation (MSG) satellites. We present early and provisional daily nadir BRDF-adjusted reflectance (NBAR) data in the visible and near-infrared MSG channels. These utilize the high temporal resolution of MSG to produce BRDF retrievals with a greatly reduced acquisition period than the comparable MODIS products while, at the same time, removing many of the angular perturbations present within the original MSG data. The NBAR data are validated against reflectance data from the MODIS instrument and in situ data gathered at a field location in Africa throughout 2008. It is found that the MSG retrievals are stable and are of high-quality across much of the SEVIRI disk while maintaining a higher temporal resolution than the MODIS BRDF products. However, a number of circumstances are discovered whereby the BRDF model is unable to function correctly with the SEVIRI observations-primarily because of an insufficient spread of angular data due to the fixed sensor location or localized cloud contamination.
C1 [Proud, Simon Richard; Fensholt, Rasmus; Rasmussen, Mads Olander] Univ Copenhagen, Dept Geosci, DK-1350 Copenhagen, Denmark.
   [Zhang, Qingling] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA.
   [Schaaf, Crystal] Univ Massachusetts, Environm Earth & Ocean Sci Dept, Boston, MA 02125 USA.
   [Shisanya, Chris] Kenyatta Univ, Dept Geog, Nairobi, Kenya.
   [Mutero, Wycliffe] Kenya Wildlife Serv, Nairobi, Kenya.
   [Mbow, Cheikh] Univ Cheikh Anta Diop, Inst Sci Environm, Dakar, Senegal.
   [Anyamba, Assaf; Pak, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Sandholt, Inge] Danish Tech Univ Space, Div Microwaves & Remote Sensing, Copenhagen, Denmark.
RP Proud, SR (reprint author), Univ Copenhagen, Dept Geosci, DK-1350 Copenhagen, Denmark.
EM srp@geo.ku.dk
RI Fensholt, Rasmus/L-7951-2014; Zhang, Qingling/H-8066-2015; Proud,
   Simon/A-4239-2015
OI Fensholt, Rasmus/0000-0003-3067-4527; Zhang,
   Qingling/0000-0001-6403-2595; Proud, Simon/0000-0003-3880-6774
FU NASA [NNX08AE94A, NNG04GP09G]
FX Part of this work was carried out while S. R. Proud was a visiting
   scientist at the Center for Remote Sensing, Boston University. C.
   Schaaf, M. Friedl, and M. Holmes are thanked for making this visit
   possible as well as for their hospitality and assistance in Boston. Q.
   Zhang is thanked for his advice and expertise with the MODIS algorithms
   while Y. Shuai is also thanked for her assistance in compiling and
   running the MODIS direct-broadcast
   bidirectional-reflectance-distribution-function code. C. Schaaf and Q.
   Zhang were supported under NASA grants NNX08AE94A and NNG04GP09G. The
   authors would like to thank the anonymous reviewers for their very
   useful thoughts and ideas on this manuscript.
NR 62
TC 5
Z9 5
U1 0
U2 31
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 2014
VL 52
IS 10
BP 6026
EP 6039
DI 10.1109/TGRS.2013.2294602
PG 14
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
   Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
   & Photographic Technology
GA AI8NC
UT WOS:000337173200003
ER

PT J
AU Jaruwatanadilok, S
   Stiles, BW
   Fore, AG
AF Jaruwatanadilok, Sermsak
   Stiles, Bryan W.
   Fore, Alexander G.
TI Cross-Calibration Between QuikSCAT and Oceansat-2
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Calibration; Oceansat-2; QuikSCAT; scatterometer
ID SCATTEROMETER MEASUREMENTS; INTERANNUAL VARIABILITY; WEATHER PREDICTION;
   WIND DATA; SEA; BACKSCATTER; MODELS; TRENDS; IMPACT
AB This paper presents the procedure to perform cross-calibration of radar backscatter between the QuikSCAT and Oceansat-2 ocean wind scatterometers. Both QuikSCAT and Oceansat-2 are Ku-band dual pencil beam, rotating antenna scatterometers with similar design. There has been a joint effort by the Indian Space Research Organization, NASA, KNMI, and NOAA to perform calibration and validation of Oceansat-2 in order to extend the climate data record of ocean surface vector winds obtained by QuikSCAT. This has resulted in significant improvement in the quality of the normalized radar cross section (NRCS) data and the quality of the resultant winds produced using the Oceansat-2 NRCS measurements. An important aspect of this calibration is the reduction of the calibration bias between QuikSCAT and Oceansat-2. The nonspinning QuikSCAT scatterometer was repointed to achieve the same incidence angles for its two HH and VV polarized antenna beams as those utilized by Oceansat-2. The magnitudes of the NRCS (backscatter) measurements of the two scatterometers were then compared for two years in order to determine NRCS bias in decibels as a function of time. Biases for both antenna beams were computed. A wind speed/wind-relative azimuth angle histogram-matched method was applied to ocean data from the two scatterometers to determine the time series of the bias between the two. It has been determined that there was an similar to 0.5 dB drop in Oceansat-2 radar backscatter on August 20, 2010. As a result, we compute cross-calibration adjustments to apply to Oceansat-2 data before and after this distinct drop in backscatter.
C1 [Jaruwatanadilok, Sermsak; Stiles, Bryan W.; Fore, Alexander G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jaruwatanadilok, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jaruwata@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This work was carried out at the Jet Propulsion Laboratory, California
   Institute of Technology, Pasadena, CA, USA, under a contract with the
   National Aeronautics and Space Administration. Government sponsorship
   acknowledged.
NR 36
TC 0
Z9 0
U1 0
U2 9
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 2014
VL 52
IS 10
BP 6197
EP 6204
DI 10.1109/TGRS.2013.2295539
PG 8
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
   Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
   & Photographic Technology
GA AI8NC
UT WOS:000337173200017
ER

PT J
AU Konings, AG
   Entekhabi, D
   Moghaddam, M
   Saatchi, SS
AF Konings, Alexandra G.
   Entekhabi, Dara
   Moghaddam, Mahta
   Saatchi, Sassan S.
TI The Effect of Variable Soil Moisture Profiles on P-Band Backscatter
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Soil moisture; stratified media; synthetic aperture radar
ID LAYERED ROUGH SURFACES; MICROWAVE EMISSION; SCATTERING; WATER;
   TEMPERATURE; SUBSURFACE; MODEL; ASSIMILATION; VARIABILITY; DYNAMICS
AB Radar measurements at P-band are sensitive to profile soil moisture. Associated backscatter measurements depend on the distribution and variation of the soil moisture profile. Existing scattering models account for this variation by approximating the soil moisture profile as consisting of a number of homogeneous layers. Since the inversion of the scattering models during the retrieval process can be based on only a few polarimetric backscatter measurements, the number of obtainable independent layers in the profile representation is limited. The purpose of this paper is to gain insights into the effects of the layering representation on the resulting modeled forward scattering. These insights form the rational basis for the design of retrieval algorithms. The effects of reflections between layers and other sources of error on simulated backscattering coefficients are first illustrated using several case studies. To determine the combined effect of different error sources for realistic soil moisture profiles, ten years of conditions at a grassland in California are studied. Depending on the layering strategy and the polarization, the root-mean-square error (RMSE) of backscattering coefficients due to misrepresenting the profile alone can be up to 2 dB, although errors can be up to 10 dB in particular cases. The error generally decreases as additional layers are added. The HH-polarization is more sensitive to the subsurface than the VV-polarization and has greater errors. Using a profile-dependent layer placement strategy decreases the RMSE of the backscatter simulation by less than 1 dB relative to a strategy with fixed layering.
C1 [Konings, Alexandra G.; Entekhabi, Dara] MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA.
   [Moghaddam, Mahta] Univ So Calif, Los Angeles, CA 90089 USA.
   [Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Konings, AG (reprint author), MIT, Dept Civil & Environm Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM konings@mit.edu
OI Konings, Alexandra/0000-0002-2810-1722
NR 48
TC 0
Z9 0
U1 1
U2 22
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 2014
VL 52
IS 10
BP 6315
EP 6325
DI 10.1109/TGRS.2013.2296035
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 AI8NC
UT WOS:000337173200026
ER

PT J
AU Sun, JQ
   Xiong, XX
   Li, YH
   Madhavan, S
   Wu, AS
   Wenny, BN
AF Sun, Junqiang
   Xiong, Xiaoxiong
   Li, Yonghong
   Madhavan, Sriharsha
   Wu, Aisheng
   Wenny, Brian N.
TI Evaluation of Radiometric Improvements With Electronic Crosstalk
   Correction for Terra MODIS Band 27
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Crosstalk; MODerate-resolution Imaging Spectroradiometer (MODIS); Moon;
   radiometric; Terra; thermal emissive bands (TEBs)
ID REFLECTIVE SOLAR BANDS; ON-ORBIT CALIBRATION; THERMAL EMISSIVE BANDS;
   PERFORMANCE; CHANNELS
AB The MODerate-resolution Imaging Spectroradiometer (MODIS) has 36 bands, covering a wavelength range from 0.4 to 14.4 mu m. Terra MODIS band 27 (6.72 mu m), a water vapor band, was found to have electronic crosstalk from other bands located on the same focal plane assembly, which causes surface feature contamination and pronounced detector level striping in the images. In a previous study, an algorithm using a linear approximation derived from on-orbit lunar observations was developed to correct the crosstalk effect. Results demonstrated that the correction substantially reduces the striping and removes the contaminated surface features. However, it was also demonstrated that the crosstalk effect might bring about a long-term increase in the brightness temperatures (BTs) in Terra band 27. In this paper, it is shown that there is a long-term drift (or decrease), which is strongly detector dependent, in the BT for the band induced by the crosstalk effect. It is also shown that the crosstalk correction with the linear algorithm substantially removes the detector-dependent long-term drift and greatly improves the radiometric accuracy of the band. The comparison between the BT of Terra band 27 in the most recent MODIS Level 1B (L1B) collection [Collection 6 (C6)] and those from the Infrared Atmospheric Sounding Interferometer using simultaneous-nadir-overpass observations shows that the detector-averaged long-term drift in the BT in Terra band 27 varies from approximately 1 K to 3 K. The detector difference can be as large as 9 K for a few detectors during the last five years in the northern and southern polar areas. With crosstalk correction applied, the long-term drift is reduced to be less than 0.5 K, and the detector difference is within 1 K. The crosstalk effect-induced detector-dependent long-term drift in Terra band 27 and the capability of the crosstalk correction algorithm to remove the drift are also assessed at three well-characterized sites with different radiance levels, namely, Dome Concordia (Dome C), Libya 1, and the Pacific Ocean at various radiometric levels. The long-term drift and the strong detector dependence of the drift are clearly observed at the three sites with the BT in the Terra band 27 C6 L1B products. The band-averaged BT drifts are about 0.8 K, 5 K, and 5.5 K, and the detector differences can be as large as 4 K, 12 K, and 15 K, respectively, for the three sites. With the crosstalk correction applied, the long-term drifts in the BT over the three sites are substantially removed, and the observed detector differences of Terra band 27 at the three sites are also significantly reduced. The crosstalk correction greatly improves the radiometric accuracy of the band as well as the image quality.
C1 [Sun, Junqiang; Li, Yonghong; Wu, Aisheng; Wenny, Brian N.] Sigma Space Corp, Lanham, MD 20706 USA.
   [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
   [Madhavan, Sriharsha] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Sun, JQ (reprint author), Sigma Space Corp, Lanham, MD 20706 USA.
NR 21
TC 16
Z9 17
U1 0
U2 12
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD OCT
PY 2014
VL 52
IS 10
BP 6497
EP 6507
DI 10.1109/TGRS.2013.2296747
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 AI8NC
UT WOS:000337173200041
ER

PT J
AU Meister, G
   Franz, BA
AF Meister, Gerhard
   Franz, Bryan A.
TI Corrections to the MODIS Aqua Calibration Derived From MODIS Aqua Ocean
   Color Products
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Calibration; image sensors; remote sensing
ID CROSS CALIBRATION; BANDS
AB Ocean color products such as, e.g., chlorophyll-a concentration, can be derived from the top-of-atmosphere radiances measured by imaging sensors on earth-orbiting satellites. There are currently three National Aeronautics and Space Administration sensors in orbit capable of providing ocean color products. One of these sensors is the Moderate Resolution Imaging Spectroradiometer (MODIS) on the Aqua satellite, whose ocean color products are currently the most widely used of the three. A recent improvement to the MODIS calibration methodology has used land targets to improve the calibration accuracy. This study evaluates the new calibration methodology and describes further calibration improvements that are built upon the new methodology by including ocean measurements in the form of global temporally averaged water-leaving reflectance measurements. The calibration improvements presented here mainly modify the calibration at the scan edges, taking advantage of the good performance of the land target trending in the center of the scan.
C1 [Meister, Gerhard; Franz, Bryan A.] NASA, Goddard Space Flight Ctr, Ocean Ecol Branch, Greenbelt, MD 20771 USA.
RP Meister, G (reprint author), NASA, Goddard Space Flight Ctr, Ocean Ecol Branch, Greenbelt, MD 20771 USA.
EM gerhard.meister@nasa.gov
RI Franz, Bryan/D-6284-2012
OI Franz, Bryan/0000-0003-0293-2082
NR 15
TC 8
Z9 8
U1 0
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 OCT
PY 2014
VL 52
IS 10
BP 6534
EP 6541
DI 10.1109/TGRS.2013.2297233
PG 8
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
   Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
   & Photographic Technology
GA AI8NC
UT WOS:000337173200044
ER

PT J
AU Roithmayr, CM
   Lukashin, C
   Speth, PW
   Kopp, G
   Thome, K
   Wielicki, BA
   Young, DF
AF Roithmayr, Carlos M.
   Lukashin, Constantine
   Speth, Paul W.
   Kopp, Greg
   Thome, Kurt
   Wielicki, Bruce A.
   Young, David F.
TI CLARREO Approach for Reference Intercalibration of Reflected Solar
   Sensors: On-Orbit Data Matching and Sampling
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Data sampling; intercalibration; orbital simulation; radiometry
ID ANGULAR-DISTRIBUTION MODELS; RADIATIVE FLUX ESTIMATION; ENERGY SYSTEM
   INSTRUMENT; INTER-CALIBRATION; PART I; MODIS; CLOUDS; TERRA; SATELLITE;
   METHODOLOGY
AB The implementation of the Climate Absolute Radiance and Refractivity Observatory (CLARREO) mission was recommended by the National Research Council in 2007 to provide an on-orbit intercalibration standard with accuracy of 0.3% (k = 2) for relevant Earth observing sensors. The goal of reference intercalibration, as established in the Decadal Survey, is to enable rigorous high-accuracy observations of critical climate change parameters, including reflected broadband radiation [Clouds and Earth's Radiant Energy System (CERES)], cloud properties [Visible Infrared Imaging Radiometer Suite (VIIRS)], and changes in surface albedo, including snow and ice albedo feedback. In this paper, we describe the CLARREO approach for performing intercalibration on orbit in the reflected solar (RS) wavelength domain. It is based on providing highly accurate spectral reflectance and reflected radiance measurements from the CLARREO Reflected Solar Spectrometer (RSS) to establish an on-orbit reference for existing sensors, namely, CERES and VIIRS on Joint Polar Satellite System satellites, Advanced Very High Resolution Radiometer and follow-on imagers on MetOp, Landsat imagers, and imagers on geostationary platforms. One of two fundamental CLARREO mission goals is to provide sufficient sampling of high-accuracy observations that are matched in time, space, and viewing angles with measurements made by existing instruments, to a degree that overcomes the random error sources from imperfect data matching and instrument noise. The data matching is achieved through CLARREO RSS pointing operations on orbit that align its line of sight with the intercalibrated sensor. These operations must be planned in advance; therefore, intercalibration events must be predicted by orbital modeling. If two competing opportunities are identified, one target sensor must be given priority over the other. The intercalibration method is to monitor changes in targeted sensor response function parameters: effective offset, gain, nonlinearity, optics spectral response, and sensitivity to polarization. In this paper, we use existing satellite data and orbital simulation methods to determine mission requirements for CLARREO, its instrument pointing ability, methodology, and needed intercalibration sampling and data matching for accurate intercalibration of RS radiation sensors on orbit. We conclude that with the CLARREO RSS in a polar 90 degrees inclination orbit at a 609-km altitude, estimated intercalibration sampling will limit the uncertainty contribution from data matching noise to 0.3% (k = 2) over the climate autocorrelation time period. The developed orbital modeling and intercalibration event prediction will serve as a framework for future mission operations.
C1 [Roithmayr, Carlos M.; Lukashin, Constantine; Speth, Paul W.; Wielicki, Bruce A.; Young, David F.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Speth, Paul W.] George Washington Univ, Washington, DC 20052 USA.
   [Kopp, Greg] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
   [Thome, Kurt] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Roithmayr, CM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM constantine.lukashin@nasa.gov
RI Thome, Kurtis/D-7251-2012; Richards, Amber/K-8203-2015
FU NASA CLARREO project
FX This work was supported by the NASA CLARREO project.
NR 31
TC 5
Z9 5
U1 3
U2 38
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 2014
VL 52
IS 10
BP 6762
EP 6774
DI 10.1109/TGRS.2014.2302397
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 AI8NC
UT WOS:000337173200063
ER

PT J
AU Zhang, B
   Orchard, M
   Saha, B
   Saxena, A
   Lee, YJ
   Vachtsevanos, G
AF Zhang, Bin
   Orchard, Marcos
   Saha, Bhaskar
   Saxena, Abhinav
   Lee, Young Jin
   Vachtsevanos, George
TI A verification framework with application to a propulsion system
SO EXPERT SYSTEMS WITH APPLICATIONS
LA English
DT Article
DE Verification; Offline verification; Runtime verification; Monte Carlo
   simulations; Propulsion systems; Automated contingency management (ACM)
ID FORMAL VERIFICATION; FAULT-DIAGNOSIS; MODEL CHECKING; IDENTIFICATION;
   ALGORITHM
AB This paper introduces a novel verification framework for Prognostics and Health Management (PHM) systems. Critical aircraft, spacecraft and industrial systems are required to perform robustly, reliably and safely. They must integrate hardware and software tools intended to detect and identify incipient failures and predict the remaining useful life (RUL) of failing components. Furthermore, it is desirable that non-catastrophic faults be accommodated, that is fault tolerant or contingency management algorithms be developed that will safeguard the operational integrity of such assets for the duration of the emergency. It is imperative, therefore, that models and algorithms designed to achieve these objectives be verified before they are validated and implemented on-board an aircraft. This paper develops a verification approach that builds upon concepts from system analysis, specification definition, system modeling, and Monte Carlo simulations. The approach is implemented in a hierarchical structure at various levels from component to system safety. Salient features of the proposed methodology are illustrated through its application to a spacecraft propulsion system. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Zhang, Bin] Univ S Carolina, Dept Elect Engn, Columbia, SC 29208 USA.
   [Orchard, Marcos] Univ Chile, Dept Elect Engn, Santiago 8370451, Chile.
   [Orchard, Marcos] Univ Chile, Adv Min Technol Ctr, Santiago 8370451, Chile.
   [Saha, Bhaskar] Xerox Corp, Palo Alto Res Ctr, Palo Alto, CA 94304 USA.
   [Saxena, Abhinav] NASA, Ames Res Ctr, Stinger Ghaffarian Technol Inc, Moffett Field, CA 94035 USA.
   [Lee, Young Jin; Vachtsevanos, George] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA.
RP Zhang, B (reprint author), Univ S Carolina, Dept Elect Engn, Columbia, SC 29208 USA.
EM zhangbin@cec.sc.edu; morchard@ing.uchile.cl; bhaskar.saha@parc.com;
   abhinav.saxena@nasa.gov; gjv@ece.gatech.edu
RI Orchard, Marcos/H-4418-2013; researchers, ac3e/N-2008-2016
OI Orchard, Marcos/0000-0003-4778-2719; 
NR 28
TC 1
Z9 1
U1 1
U2 27
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0957-4174
EI 1873-6793
J9 EXPERT SYST APPL
JI Expert Syst. Appl.
PD OCT 1
PY 2014
VL 41
IS 13
BP 5669
EP 5679
DI 10.1016/j.eswa.2014.03.017
PG 11
WC Computer Science, Artificial Intelligence; Engineering, Electrical &
   Electronic; Operations Research & Management Science
SC Computer Science; Engineering; Operations Research & Management Science
GA AI4YJ
UT WOS:000336872300002
ER

PT J
AU Nieves, V
   Wang, J
   Willis, JK
AF Nieves, V.
   Wang, J.
   Willis, J. K.
TI A conceptual model of ocean freshwater flux derived from sea surface
   salinity
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID GROUND HEAT-FLUX; TEMPERATURE; LAYER; PRECIPITATION; CIRCULATION;
   EVAPORATION; DIFFUSION; SPACE
AB A conceptual model is proposed to express freshwater flux (evaporation minus precipitation) as a function of sea surface salinity (and vice versa). The model is formulated using an idealized one-dimensional diffusion equation for the ocean surface layer. It is shown to provide good agreement with existing freshwater flux estimates and salinity observations. It also has the potential to enhance our capability of monitoring and modeling global freshwater fluxes and salinity as a data retrieval algorithm for remote sensing. The model may improve physical parameterization in coupled ocean-atmosphere models to study the global water cycle.
C1 [Nieves, V.; Willis, J. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
   [Wang, J.] Georgia Inst Technol, Atlanta, GA 30332 USA.
RP Nieves, V (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM veronica.nieves@jpl.nasa.gov
FU NSF [EAR-1138611]; ARO [W911NF-10-1-0236/W911NF-12-1-0095]
FX The research described in this paper was carried out at the Jet
   Propulsion Laboratory, California Institute of Technology. This work was
   supported by NSF EAR-1138611 and ARO W911NF-10-1-0236/W911NF-12-1-0095
   grants. ECCO2 data are provided by D. Menemenlis and H. Zhang.
NR 21
TC 0
Z9 0
U1 2
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD SEP 28
PY 2014
VL 41
IS 18
BP 6452
EP 6458
DI 10.1002/2014GL061365
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA AT4MO
UT WOS:000344913700019
ER

PT J
AU Efremova, B
   McIntire, J
   Moyer, D
   Wu, AS
   Xiong, XX
AF Efremova, Boryana
   McIntire, Jeff
   Moyer, David
   Wu, Aisheng
   Xiong, Xiaoxiong
TI S-NPP VIIRS thermal emissive bands on-orbit calibration and performance
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID PRODUCTS
AB Presented is an assessment of the on-orbit radiometric performance of the thermal emissive bands (TEB) of the Suomi National Polar-orbiting Partnership (S-NPP) Visible Infrared Imaging Radiometer Suite (VIIRS) instrument based on data from the first 2 years of operations-from 20 January 2012 to 20 January 2014. The VIIRS TEB are calibrated on orbit using a V-grooved blackbody (BB) as a radiance source. Performance characteristics trended over the life of the mission include the F factor-a measure of the gain change of the TEB detectors; the Noise Equivalent differential Temperature (NEdT)-a measure of the detector noise; and the detector offset and nonlinear terms trended at the quarterly performed BB warm-up cool-down cycles. We find that the BB temperature is well controlled and stable within the 30mK requirement. The F factor trends are very stable and showing little degradation (within 0.8%). The offsets and nonlinearity terms are also without noticeable drifts. NEdT is stable and does not show any trend. Other TEB radiometric calibration-related activities discussed include the on-orbit assessment of the response versus scan-angle functions and an approach to improve the M13 low-gain calibration using onboard lunar measurements. We conclude that all the assessed parameters comply with the requirements, and the TEB provide radiometric measurements with the required accuracy.
C1 [Efremova, Boryana; McIntire, Jeff; Wu, Aisheng] Sigma Space Corp, Lanham, MD 20706 USA.
   [Moyer, David] Aerosp Corp, El Segundo, CA 90245 USA.
   [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Efremova, B (reprint author), Sigma Space Corp, Lanham, MD 20706 USA.
EM boryana.efremova@sigmaspace.com
NR 15
TC 9
Z9 9
U1 0
U2 3
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 2014
VL 119
IS 18
BP 10859
EP 10875
DI 10.1002/2014JD022078
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS1PO
UT WOS:000344052800016
ER

PT J
AU Ban-Weiss, GA
   Jin, L
   Bauer, SE
   Bennartz, R
   Liu, XH
   Zhang, K
   Ming, Y
   Guo, H
   Jiang, JH
AF Ban-Weiss, George A.
   Jin, Ling
   Bauer, Susanne E.
   Bennartz, Ralf
   Liu, Xiaohong
   Zhang, Kai
   Ming, Yi
   Guo, Huan
   Jiang, Jonathan H.
TI Evaluating clouds, aerosols, and their interactions in three global
   climate models using satellite simulators and observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID COMMUNITY ATMOSPHERE MODEL; GENERAL-CIRCULATION MODEL; LARGE-SCALE
   MODELS; STRATIFORM CLOUDS; DROPLET FORMATION; MICROPHYSICAL PROPERTIES;
   INTERCOMPARISON PROJECT; INSTRUMENT SIMULATORS; RADIATIVE PROPERTIES;
   SOUTHEAST PACIFIC
AB Accurately representing aerosol-cloud interactions in global climate models is challenging. As parameterizations evolve, it is important to evaluate their performance with appropriate use of observations. In this investigation we compare aerosols, clouds, and their interactions in three global climate models (Geophysical Fluid Dynamics Laboratory-Atmosphere Model 3 (AM3), National Center for Atmospheric Research-Community Atmosphere Model 5 (CAM5), and Goddard Institute for Space Studies-ModelE2) to Aqua Moderate Resolution Imaging Spectroradiometer (MODIS) satellite observations. Modeled cloud properties are diagnosed using a MODIS simulator. Cloud droplet number concentrations (N) are computed identically from satellite-simulated and MODIS-observed values of liquid cloud optical depth and droplet effective radius. We find that aerosol optical depth (tau(a)) simulated by models is similar to observations in many regions around the globe. For N, AM3 and CAM5 capture the observed spatial pattern of higher values in coastal marine stratocumulus versus remote ocean regions, though modeled values, in general, are higher than observed. Aerosol-cloud interactions were computed as the sensitivity of ln(N) to ln(tau(a)) for coastal marine liquid clouds near South Africa (SAF) and Southeast Asia where tau(a) varies in time. AM3 and CAM5 are more sensitive than observations, while the sensitivity for ModelE2 is statistically insignificant. This widely used sensitivity could be subject to misinterpretation due to the confounding influence of meteorology on both aerosols and clouds. A simple framework for assessing the sensitivity of ln(N) to ln(tau(a)) at constant meteorology illustrates that observed sensitivity can change from positive to statistically insignificant when including the confounding influence of relative humidity. Satellite-simulated versus standard model values of N are compared; for CAM5 in SAF, standard model values are significantly lower than satellite-simulated values with a bias of 83 cm(-3).
C1 [Ban-Weiss, George A.] Univ So Calif, Los Angeles, CA 90089 USA.
   [Jin, Ling] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
   [Bauer, Susanne E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
   [Bauer, Susanne E.] Columbia Univ, Earth Inst, New York, NY USA.
   [Bennartz, Ralf] Vanderbilt Univ, Dept Earth & Environm Sci, Nashville, TN 37235 USA.
   [Bennartz, Ralf] Univ Wisconsin, Madison, WI USA.
   [Liu, Xiaohong] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA.
   [Liu, Xiaohong; Zhang, Kai] Pacific NW Natl Lab, Atmospher Sci & Global Change Div, Richland, WA 99352 USA.
   [Ming, Yi] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
   [Guo, Huan] NOAA, UCAR Visiting Scientist Programs, Geophys Fluid Dynam Lab, Princeton, NJ USA.
   [Jiang, Jonathan H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Ban-Weiss, GA (reprint author), Univ So Calif, Los Angeles, CA 90089 USA.
EM banweiss@usc.edu
RI Liu, Xiaohong/E-9304-2011; Bauer, Susanne/P-3082-2014; Ming,
   Yi/F-3023-2012; Zhang, Kai/F-8415-2010; 
OI Liu, Xiaohong/0000-0002-3994-5955; Zhang, Kai/0000-0003-0457-6368;
   Ban-Weiss, George/0000-0001-8211-2628
FU Department of Energy's (DOE) Earth System Modeling (ESM) Program via the
   FASTER (FAst-physics System TEstbed and Research) project; NASA MAP
   program Modeling, Analysis, and Prediction Climate Variability and
   Change [NNH08ZDA001N-MAP]; Office of Science of U.S. Department of
   Energy as part of the Earth System Modeling Program; DOE SciDAC program
   on Applying Computationally Efficient Schemes for BioGeochemical Cycles
   [ACES4BGC]; Jet Propulsion Laboratory, California Institute of
   Technology, under NASA; U.S. Department of Energy's Earth System
   Modeling, an Office of Science, Office of Biological and Environmental
   Research program [DE-AC02-05CH11231]; DOE by Battelle Memorial Institute
   [DE-AC06-76RLO 1830]; NCAR's Computational and Information Systems
   Laboratory
FX MODIS observations supporting Figures 1-5 and 8 are freely available
   from National Aeronautics and Space Administration. Global climate model
   data used for these figures may be made available upon request from the
   corresponding author. Data supporting Figures 6 and 7 can be found in
   the supporting information. The ERA-Interim reanalysis data are freely
   available from European Centre for Medium-Range Weather Forecasts.
   G.B.W. and S.B. were supported by the Department of Energy's (DOE) Earth
   System Modeling (ESM) Program via the FASTER (FAst-physics System
   TEstbed and Research) project. L.J. was supported by the NASA MAP
   program Modeling, Analysis, and Prediction Climate Variability and
   Change (NNH08ZDA001N-MAP). X. L. and K.Z. were supported by the Office
   of Science of U.S. Department of Energy as part of the Earth System
   Modeling Program and the DOE SciDAC program on Applying Computationally
   Efficient Schemes for BioGeochemical Cycles (ACES4BGC). J.H.J. was
   supported by the Jet Propulsion Laboratory, California Institute of
   Technology, under contract by NASA. Work at Lawrence Berkeley National
   Laboratory was also supported by the U.S. Department of Energy's Earth
   System Modeling, an Office of Science, Office of Biological and
   Environmental Research program under contract DE-AC02-05CH11231. The
   Pacific Northwest National Laboratory is operated for DOE by Battelle
   Memorial Institute under contract DE-AC06-76RLO 1830. X. L. would like
   to acknowledge the use of computational resources (ark:/85065/ d7wd3xhc)
   at the NCAR-Wyoming Supercomputing Center provided by the National
   Science Foundation and the State of Wyoming and supported by NCAR's
   Computational and Information Systems Laboratory. S. B. acknowledges
   resources supporting this work by the NASA High-End Computing (HEC)
   Program through the NASA Center for Climate Simulation (NCCS) at Goddard
   Space Flight Center. For helpful discussions and guidance, we thank
   Surabi Menon (formerly of Lawrence Berkeley National Laboratory), David
   Romps and William Collins (Lawrence Berkeley National Laboratory and
   University of California, Berkeley), Gijs de Boer and Robert Pincus
   (NOAA Earth System Research Laboratory), Jennifer Kay (National Center
   for Atmospheric Research), and Yangang Liu (Brookhaven National
   Laboratory). We acknowledge the MODIS Science Team for processing and
   making publically available the satellite data used in this study. We
   also acknowledge ECMWF for the ERA-Interim reanalysis.
NR 106
TC 6
Z9 6
U1 0
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 2014
VL 119
IS 18
BP 10876
EP 10901
DI 10.1002/2014JD021722
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS1PO
UT WOS:000344052800017
ER

PT J
AU Homeyer, CR
   Pan, LL
   Dorsi, SW
   Avallone, LM
   Weinheimer, AJ
   O'Brien, AS
   DiGangi, JP
   Zondlo, MA
   Ryerson, TB
   Diskin, GS
   Campos, TL
AF Homeyer, Cameron R.
   Pan, Laura L.
   Dorsi, Samuel W.
   Avallone, Linnea M.
   Weinheimer, Andrew J.
   O'Brien, Anthony S.
   DiGangi, Joshua P.
   Zondlo, Mark A.
   Ryerson, Thomas B.
   Diskin, Glenn S.
   Campos, Teresa L.
TI Convective transport of water vapor into the lower stratosphere observed
   during double-tropopause events
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID DIODE-LASER HYGROMETER; EXTRATROPICAL TROPOPAUSE; MIDLATITUDE
   CONVECTION; SATELLITE-OBSERVATIONS; TROPOSPHERE EXCHANGE;
   BOUNDARY-LAYER; FAST-RESPONSE; RESOLUTION; TOP; AIRCRAFT
AB We present in situ observations of convectively injected water vapor in the lower stratosphere from instruments aboard two aircraft operated during the Deep Convective Clouds and Chemistry experiment. Water vapor mixing ratios in the injected air are observed to be 60-225 ppmv at altitudes 1-2 km above the tropopause (350-370 K potential temperature), well above observed background mixing ratios of 5-10 ppmv in the lower stratosphere. Radar observations of the responsible convective systems show deep overshooting at altitudes up to 4 km above the lapse rate tropopause and above the flight ceilings of the aircraft. Backward trajectories from the in situ observations show that convectively injected water vapor is observed from three distinct types of systems: isolated convection, a convective line, and a leading line-trailing stratiform mesoscale convective system. Significant transport of additional tropospheric or boundary layer trace gases is observed only for the leading line-trailing stratiform case. In addition, all observations of convective injection are found to occur within large-scale double-tropopause events from poleward Rossby wave breaking. Based on this relationship, we present a hypothesis on the role of the large-scale lower stratosphere during convective overshooting. In particular, the reduced lower stratosphere stability associated with double-tropopause environments may facilitate deeper levels of overshooting and convective injection.
C1 [Homeyer, Cameron R.; Pan, Laura L.; Weinheimer, Andrew J.; Campos, Teresa L.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
   [Dorsi, Samuel W.; Avallone, Linnea M.] Univ Colorado, Dept Atmospher & Ocean Sci, LASP, Boulder, CO 80309 USA.
   [O'Brien, Anthony S.; DiGangi, Joshua P.; Zondlo, Mark A.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
   [DiGangi, Joshua P.; Diskin, Glenn S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
   [Ryerson, Thomas B.] NOAA, Chem Sci Div, ESRL, Boulder, CO USA.
RP Homeyer, CR (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
EM chomeyer@ou.edu
RI Homeyer, Cameron/D-5034-2013; Pan, Laura/A-9296-2008; Ryerson,
   Tom/C-9611-2009; Zondlo, Mark/R-6173-2016
OI Homeyer, Cameron/0000-0002-4883-6670; Pan, Laura/0000-0001-7377-2114;
   Zondlo, Mark/0000-0003-2302-9554
FU National Science Foundation
FX The National Center for Atmospheric Research is sponsored by the
   National Science Foundation. We acknowledge the DC3 science team for
   access to the aircraft data and motivation for this study. We also thank
   Eric Jensen, John Bergman, Marta Abalos, Mike Fromm, and two anonymous
   reviewers for their helpful comments and suggestions. The first author
   also thanks the Advanced Study Program (ASP) at NCAR for Postdoctoral
   support. All data used in this study are free and publicly available.
   DC3 aircraft observations and NWS radiosondes were attained at
   https://www.eol. ucar. edu/field_ projects/dc3/,NCEP-GFS analyses at
   http://nomads.ncdc.noaa.gov/, NEXRAD WSR-88D radar observations at
   http://has. ncdc. noaa. gov/, DOE-ARM radiosondes at http://www.
   archive. arm. gov/, and Oklahoma Mesonet observations at https://www.
   mesonet. org.
NR 60
TC 18
Z9 18
U1 3
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 SEP 27
PY 2014
VL 119
IS 18
BP 10941
EP 10958
DI 10.1002/2014JD021485
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS1PO
UT WOS:000344052800021
ER

PT J
AU Haskins, JB
   Bennett, WR
   Wu, JJ
   Hernandez, DM
   Borodin, O
   Monk, JD
   Bauschlicher, CW
   Lawson, JW
AF Haskins, Justin B.
   Bennett, William R.
   Wu, James J.
   Hernandez, Dionne M.
   Borodin, Oleg
   Monk, Joshua D.
   Bauschlicher, Charles W., Jr.
   Lawson, John W.
TI Computational and Experimental Investigation of Li-Doped Ionic Liquid
   Electrolytes: [pyr14][TFSI], [pyr13][FSI], and [EMIM][BF4]
SO JOURNAL OF PHYSICAL CHEMISTRY B
LA English
DT Article
ID MOLECULAR-DYNAMICS SIMULATIONS; BIS(TRIFLUOROMETHANESULFONYL) IMIDE
   ANION; POLARIZABLE FORCE-FIELDS; LITHIUM METAL-ELECTRODES;
   BIS(FLUOROSULFONYL) IMIDE; TRANSPORT-PROPERTIES; ELECTROCHEMICAL
   PROPERTIES; PHYSICOCHEMICAL PROPERTIES; PYRROLIDINIUM CATIONS;
   RAMAN-SPECTROSCOPY
AB We employ molecular dynamics (MD) simulation and experiment to investigate the structure, thermodynamics, and transport of N-methyl-N-butylpyrrolidinium bis(trifluoromethylsufonyl)imide ([pyr14][TESI]), N-methyl-N-propylpyrrolidinium bis (fluorosufonyl)imide ([pyr13][FSI]), and 1-ethyl-3-methylimidazolium boron tetrafluoride ([EMIM][BF4]), as a function of Li-salt mole fraction (0.05 <= x(Li+) <= 0.33) and temperature (298 K <= T <= 393 K). Structurally, Li+ is shown to be solvated by three anion neighbors in [pyr14][TFSI] and four anion neighbors in both [pyr13][FSI] and [EMIM][BF4], and at all levels of x(Li+) we find the presence of lithium aggregates. Pulsed field gradient spin-echo NMR measurements of diffusion and electrochemical impedance spectroscopy measurements of ionic conductivity are made for the neat ionic liquids as well as 0.5 molal solutions of Li-salt in the ionic liquids. Bulk ionic liquid properties (density, diffusion, viscosity, and ionic conductivity) are obtained with MD simulations and show excellent agreement with experiment. While the diffusion exhibits a systematic decrease with increasing x(Li+), the contribution of Li+ to ionic conductivity increases until reaching a saturation doping level of x(Li+) = 0.10. Comparatively, the Li+ conductivity of [pyr14][TFSI] is an order of magnitude lower than that of the other liquids, which range between 0.1 and 0.3 mS/cm. Our transport results also demonstrate the necessity of long MD simulation runs (similar to 200 ns) to converge transport properties at room temperature. The differences in Li+ transport are reflected in the residence times of Li+ with the anions (tau(Li+/-)), which are revealed to be much larger for [pyr14][TESI] (up to 100 ns at the highest doping levels) than in either [EMIM][BF4] or [pyr13][FSI]. Finally, to comment on the relative kinetics of Li+ transport in each liquid, we find that while the net motion of Li+ with its solvation shell (vehicular) significantly contributes to net diffusion in all liquids, the importance of transport through anion exchange increases at high x(Li+) and in liquids with large anions.
C1 [Haskins, Justin B.; Monk, Joshua D.] NASA, ERC Inc, Thermal Protect Mat & Syst Branch, Moffett Field, CA 94035 USA.
   [Bauschlicher, Charles W., Jr.] NASA, Entry Syst & Technol Div, Moffett Field, CA 94035 USA.
   [Lawson, John W.] NASA, Thermal Protect Mat & Syst Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Bennett, William R.; Wu, James J.; Hernandez, Dionne M.] NASA, Electrochem Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
   [Borodin, Oleg] US Army Res Lab, Electrochem Branch, Sensor & Electron Devices Directorate, Adelphi, MD 20783 USA.
RP Lawson, JW (reprint author), NASA, Thermal Protect Mat & Syst Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM john.w.lawson@nasa.gov
RI Borodin, Oleg/B-6855-2012
OI Borodin, Oleg/0000-0002-9428-5291
FU NASA Aeronautics Research Institute (NARI) Seedling program
FX This work was supported by funding from the NASA Aeronautics Research
   Institute (NARI) Seedling program.
NR 61
TC 22
Z9 22
U1 9
U2 78
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1520-6106
J9 J PHYS CHEM B
JI J. Phys. Chem. B
PD SEP 25
PY 2014
VL 118
IS 38
BP 11295
EP 11309
DI 10.1021/jp5061705
PG 15
WC Chemistry, Physical
SC Chemistry
GA AP9JL
UT WOS:000342396000027
PM 25159701
ER

PT J
AU Fraine, J
   Deming, D
   Benneke, B
   Knutson, H
   Jordan, A
   Espinoza, N
   Madhusudhan, N
   Wilkins, A
   Todorov, K
AF Fraine, Jonathan
   Deming, Drake
   Benneke, Bjorn
   Knutson, Heather
   Jordan, Andres
   Espinoza, Nestor
   Madhusudhan, Nikku
   Wilkins, Ashlee
   Todorov, Kamen
TI Water vapour absorption in the clear atmosphere of a Neptune-sized
   exoplanet
SO NATURE
LA English
DT Article
ID HUBBLE-SPACE-TELESCOPE; SUPER-EARTHS; TRANSMISSION SPECTROSCOPY;
   EXTRASOLAR PLANETS; MINI-NEPTUNES; LIGHT CURVES; HD 189733B; C/O RATIO;
   GJ 436B; TRANSITS
AB Transmission spectroscopy has so far detected atomic and molecular absorption in Jupiter-sized exoplanets, but intense efforts to measure molecular absorption in the atmospheres of smaller (Neptune-sized) planets during transits have revealed only featureless spectra(1-4). From this it was concluded that the majority of small, warm planets evolve to sustain atmospheres with high mean molecular weights (little hydrogen), opaque clouds or scattering hazes, reducing our ability to observe the composition of these atmospheres(1-5). Here we report observations of the transmission spectrum of the exoplanet HAT-P-11b (which has a radius about four times that of Earth) from the optical wavelength range to the infrared. We detected water vapour absorption at a wavelength of 1.4 micrometres. The amplitude of the water absorption (approximately 250 parts per million) indicates that the planetary atmosphere is predominantly clear down to an altitude corresponding to about 1 millibar, and sufficiently rich in hydrogen to have a large scale height (over which the atmospheric pressure varies by a factor of e). The spectrum is indicative of a planetary atmosphere in which the abundance of heavy elements is no greater than about 700 times the solar value. This is in good agreement with the core-accretion theory of planet formation, in which a gas giant planet acquires its atmosphere by accreting hydrogen-rich gas directly from the protoplanetary nebula onto a large rocky or icy core(6).
C1 [Fraine, Jonathan; Deming, Drake; Wilkins, Ashlee] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Fraine, Jonathan; Jordan, Andres; Espinoza, Nestor] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile.
   [Fraine, Jonathan; Benneke, Bjorn; Knutson, Heather] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
   [Deming, Drake] NASA, Astrobiol Inst Virtual Planetary Lab, Seattle, WA 98195 USA.
   [Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
   [Todorov, Kamen] Swiss Fed Inst Technol, Dept Phys, CH-8049 Zurich, Switzerland.
RP Fraine, J (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM jfraine@astro.umd.edu
OI Todorov, Kamen/0000-0002-9276-8118; Jordan, Andres/0000-0002-5389-3944
FU 'Millennium Institute of Astrophysics (MAS)' of the Millennium Science
   Initiative, Chilean Ministry of Economy [IC120009]; FONDECYT [1130857];
   BASAL CATA [PFB-06]; CONICYT-PCHA/Doctorado Nacional
FX J.F., A.J. and N.E. acknowledge support from project IC120009
   'Millennium Institute of Astrophysics (MAS)' of the Millennium Science
   Initiative, Chilean Ministry of Economy; FONDECYT project 1130857; and
   BASAL CATA PFB-06. N.E. is supported by CONICYT-PCHA/Doctorado Nacional.
   We thank P. McCullough for his assistance in the planning and execution
   of our observations. We are grateful to I. Crossfield, L. Kreidberg and
   E. Agol for providing their open-source, Python code banks on their
   individual websites. We are also grateful for discussions with M. Line,
   J. Fortney and J. Moses about the nature of photochemistry and interior
   structures. We thank the ATLAS and PHOENIX teams for providing stellar
   models. We also thank the SciPy and NumPy associations for providing
   extensive and rigorous numerical routines for an assortment of
   mathematical and computational techniques.
NR 46
TC 45
Z9 45
U1 5
U2 31
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 25
PY 2014
VL 513
IS 7519
BP 526
EP +
DI 10.1038/nature13785
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AP4VB
UT WOS:000342075800035
PM 25254473
ER

PT J
AU Kang, D
   Rim, T
   Baek, CK
   Meyyappan, M
   Lee, JS
AF Kang, Daegun
   Rim, Taiuk
   Baek, Chang-Ki
   Meyyappan, M.
   Lee, Jeong-Soo
TI Thermally Phase-Transformed In2Se3 Nanowires for Highly Sensitive
   Photodetectors
SO SMALL
LA English
DT Article
DE indium selenide; In2Se3; -phase; -phase; photodetectors
ID THIN-FILMS; OPTICAL-PROPERTIES; SILICON NANOWIRES; HEAT-TREATMENT;
   PERFORMANCE; NANOSTRUCTURES; INDIUM; SEMICONDUCTOR; ELECTRONICS; SENSORS
AB The photoresponse characteristics of In2Se3 nanowire photodetectors with the -phase and -phase structures are investigated. The as-grown -phase In2Se3 nanowires by the vapor-liquid-solid technique are phase-transformed to the -phase nanowires by thermal annealing. The photoresponse performances of the -phase and -phase In2Se3 nanowire photodetectors are characterized over a wide range of wavelengths (300-900 nm). The phase of the nanowires is analyzed using a high-resolution transmission microscopy equipped with energy dispersive X-ray spectroscopy and X-ray diffraction. The electrical conductivity and photoresponse characteristics are significantly enhanced in the -phase due to smaller bandgap structure compared to the -phase nanowires. The spectral responsivities of the -phase devices are 200 times larger than those of the -phase devices. The superior performance of the thermally phase-transformed In2Se3 nanowire devices offers an avenue to develop highly sensitive photodetector applications.
C1 [Kang, Daegun] Pohang Univ Sci & Technol, Dept Elect Engn, Pohang 790784, Gyeongbuk, South Korea.
   [Rim, Taiuk; Baek, Chang-Ki] Pohang Univ Sci & Technol, Creat IT Engn, Pohang 790784, Gyeongbuk, South Korea.
   [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Lee, Jeong-Soo] Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang 790784, Gyeongbuk, South Korea.
RP Lee, JS (reprint author), Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang 790784, Gyeongbuk, South Korea.
EM ljs6951@postech.ac.kr
FU National Research Foundation (NRF) [2012R1A2A2A02010432]; center for
   advanced soft electronics under the global frontier research program of
   the Ministry of Education, Science, and Technology (MEST)
   [2011-0031638]; IT Consilience Creative Program
   [NIPA-2013-H0203-13-1001]
FX This work was in part supported by National Research Foundation (NRF)
   (No. 2012R1A2A2A02010432) and by a grant (Code No. 2011-0031638) from
   the center for advanced soft electronics under the global frontier
   research program of the Ministry of Education, Science, and Technology
   (MEST), and by the "IT Consilience Creative Program"
   (NIPA-2013-H0203-13-1001) supervised by the National IT Industry
   Promotion Agency, Korea.
NR 47
TC 3
Z9 3
U1 12
U2 56
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA POSTFACH 101161, 69451 WEINHEIM, GERMANY
SN 1613-6810
EI 1613-6829
J9 SMALL
JI Small
PD SEP 24
PY 2014
VL 10
IS 18
BP 3795
EP 3802
DI 10.1002/smll.201400373
PG 8
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
   Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied;
   Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
   Physics
GA AQ3JF
UT WOS:000342687700027
PM 24828147
ER

PT J
AU Verma, VB
   Korzh, B
   Bussieres, F
   Horansky, RD
   Lita, AE
   Marsili, F
   Shaw, MD
   Zbinden, H
   Mirin, RP
   Nam, SW
AF Verma, V. B.
   Korzh, B.
   Bussieres, F.
   Horansky, R. D.
   Lita, A. E.
   Marsili, F.
   Shaw, M. D.
   Zbinden, H.
   Mirin, R. P.
   Nam, S. W.
TI High-efficiency WSi superconducting nanowire single-photon detectors
   operating at 2.5 K
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID TIME
AB We investigate the operation of WSi superconducting nanowire single-photon detectors (SNSPDs) at 2.5 K, a temperature which is similar to 70% of the superconducting transition temperature (T-C) of 3.4 K. We demonstrate saturation of the system detection efficiency at 78 +/- 2% at a wavelength of 1310 nm, with a jitter of 191 ps. We find that the jitter at 2.5 K is limited by the noise of the readout and can be improved through the use of cryogenic amplifiers. Operation of SNSPDs with high efficiency at temperatures very close to TC appears to be a unique property of amorphous WSi. (C) 2014 AIP Publishing LLC.
C1 [Verma, V. B.; Horansky, R. D.; Lita, A. E.; Mirin, R. P.; Nam, S. W.] NIST, Boulder, CO 80305 USA.
   [Korzh, B.; Bussieres, F.; Zbinden, H.] Univ Geneva, Grp Appl Phys, CH-1211 Geneva 4, Switzerland.
   [Marsili, F.; Shaw, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Verma, VB (reprint author), NIST, 325 Broadway, Boulder, CO 80305 USA.
RI Bussieres, Felix/E-5384-2011; 
OI Bussieres, Felix/0000-0003-0234-175X; Mirin, Richard/0000-0002-4472-4655
NR 12
TC 17
Z9 17
U1 4
U2 19
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
   MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD SEP 22
PY 2014
VL 105
IS 12
AR 122601
DI 10.1063/1.4896045
PG 3
WC Physics, Applied
SC Physics
GA AQ7NL
UT WOS:000343004400053
ER

PT J
AU Tombesi, F
   Tazaki, F
   Mushotzky, RF
   Ueda, Y
   Cappi, M
   Gofford, J
   Reeves, JN
   Guainazzi, M
AF Tombesi, F.
   Tazaki, F.
   Mushotzky, R. F.
   Ueda, Y.
   Cappi, M.
   Gofford, J.
   Reeves, J. N.
   Guainazzi, M.
TI Ultrafast outflows in radio-loud active galactic nuclei
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; line: identification;
   plasmas; galaxies: active; X-rays: galaxies
ID X-RAY-SPECTRUM; SHELL ABSORPTION-LINES; HIGH-VELOCITY OUTFLOWS; HOLE
   ACCRETION DISKS; SPINNING BLACK-HOLE; GALAXY 3C 445; XMM-NEWTON; SUZAKU
   VIEW; SEYFERT-GALAXIES; WARM ABSORBERS
AB Recent X-ray observations show absorbing winds with velocities up to mildly relativistic values of the order of similar to 0.1c in a limited sample of six broad-line radio galaxies. They are observed as blueshifted Fe XXV-XXVI K-shell absorption lines, similarly to the ultrafast outflows (UFOs) reported in Seyferts and quasars. In this work we extend the search for such Fe K absorption lines to a larger sample of 26 radio-loud active galactic nuclei (AGN) observed with XMM-Newton and Suzaku. The sample is drawn from the Swift Burst Alert Telescope 58-month catalogue and blazars are excluded. X-ray bright Fanaroff-Riley Class II radio galaxies constitute the majority of the sources. Combining the results of this analysis with those in the literature we find that UFOs are detected in > 27 per cent of the sources. However, correcting for the number of spectra with insufficient signal-to-noise ratio, we can estimate that the incidence of UFOs is this sample of radio-loud AGN is likely in the range f similar or equal to (50 +/- 20) per cent. A photoionization modelling of the absorption lines with XSTAR allows us to estimate the distribution of their main parameters. The observed outflow velocities are broadly distributed between v(out) less than or similar to 1000 km s(-1) and v(out) similar or equal to 0.4c, with mean and median values of v(out) similar or equal to 0.133c and v(out) similar or equal to 0.117c, respectively. The material is highly ionized, with an average ionization parameter of log xi similar or equal to 4.5 erg s(-1) cm, and the column densities are larger than N-H > 10(22) cm(-2). Overall, these characteristics are consistent with the presence of complex accretion disc winds in a significant fraction of radio-loud AGN and demonstrate that the presence of relativistic jets does not preclude the existence of winds, in accordance with several theoretical models.
C1 [Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
   [Tombesi, F.; Mushotzky, R. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Tazaki, F.; Ueda, Y.] Kyoto Univ, Dept Astron, Kyoto 6068502, Japan.
   [Cappi, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
   [Gofford, J.; Reeves, J. N.] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England.
   [Reeves, J. N.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
   [Guainazzi, M.] European Space Astron Ctr ESA, E-28691 Madrid, Spain.
RP Tombesi, F (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
EM ftombesi@astro.umd.edu
RI XRAY, SUZAKU/A-1808-2009; 
OI Cappi, Massimo/0000-0001-6966-8920
FU National Aeronautics and Space Administration (NASA) through
   Astrophysics Data Analysis Program, part of the ROSES [NNX12AH40G]
FX FT would like to thank R. M. Sambruna for her contribution to the
   initial definition of the project and for the comments to the
   manuscript. FT thanks C. S. Reynolds and G. M. Madejski for the useful
   discussions. 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.
NR 118
TC 22
Z9 23
U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 21
PY 2014
VL 443
IS 3
BP 2154
EP 2182
DI 10.1093/mnras/stu1297
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ6KL
UT WOS:000342920400021
ER

PT J
AU Clementel, N
   Madura, TI
   Kruip, CJH
   Icke, V
   Gull, TR
AF Clementel, N.
   Madura, T. I.
   Kruip, C. J. H.
   Icke, V.
   Gull, T. R.
TI 3D radiative transfer in eta Carinae: application of the SIMPLEX
   algorithm to 3D SPH simulations of binary colliding winds
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiative transfer; binaries: close; stars: individual: Eta Carinae;
   stars: mass-loss; stars: winds, outflows
ID RAY LIGHT-CURVE; PERIASTRON PASSAGE; PINWHEEL NEBULA; EMISSION-LINES;
   MASS-LOSS; STAR; VARIABILITY; SPECTROSCOPY; ENVIRONMENT; HOMUNCULUS
AB Eta Carinae is an ideal astrophysical laboratory for studying massive binary interactions and evolution, and stellar wind-wind collisions. Recent three-dimensional (3D) simulations set the stage for understanding the highly complex 3D flows in. Car eta Observations of different broad high-and low-ionization forbidden emission lines provide an excellent tool to constrain the orientation of the system, the primary's mass-loss rate, and the ionizing flux of the hot secondary. In this work, we present the first steps towards generating synthetic observations to compare with available and future HST/STIS data. We present initial results from full 3D radiative transfer simulations of the interacting winds in eta Car. We use the SIMPLEX algorithm to post-process the output from 3D smoothed particle hydrodynamics (SPH) simulations and obtain the ionization fractions of hydrogen and helium assuming three different mass-loss rates for the primary star. The resultant ionization maps of both species constrain the regions where the observed forbidden emission lines can form. Including collisional ionization is necessary to achieve a better description of the ionization states, especially in the areas shielded from the secondary's radiation. We find that reducing the primary's mass-loss rate increases the volume of ionized gas, creating larger areas where the forbidden emission lines can form. We conclude that post-processing 3D SPH data with SIMPLEX is a viable tool to create ionization maps for eta Car.
C1 [Clementel, N.; Kruip, C. J. H.; Icke, V.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
   [Madura, T. I.; Gull, T. R.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Clementel, N (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM clementel@strw.leidenuniv.nl
FU NASA [NAS 5-26555]; NASA through Space Telescope Science Institute
   [12013, 12508, 12750, 13054, 13395]
FX TIM 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. Support for TRG was through
   programs #12013, 12508, 12750, 13054, and 13395, provided by NASA
   through a grant from the Space Telescope Science Institute, which is
   operated by the Association of Universities for Research in Astronomy,
   Inc., under NASA contract NAS 5-26555.
NR 56
TC 6
Z9 6
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 21
PY 2014
VL 443
IS 3
BP 2475
EP 2491
DI 10.1093/mnras/stu1287
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ6KL
UT WOS:000342920400044
ER

PT J
AU Yao, HM
   Wright, MW
   Marciante, JR
AF Yao, Haomin
   Wright, Malcolm W.
   Marciante, John R.
TI Analysis of nonlinear optical and dynamic gain effects of
   moderate-power, pulse-position-modulated, erbium-doped fiber amplifiers
   for deep-space applications
SO APPLIED OPTICS
LA English
DT Article
ID SCATTERING; SYSTEM; RAMAN
AB Lasers for use in deep-space applications such as interplanetary optical communications employ multiwatt resonantly pumped dual-clad erbium-doped fiber amplifiers and the pulse-position modulation scheme. Nonlinear optical effects and dynamic gain effects often impair their performance and limit their operational range. These effects are analyzed theoretically and numerically with a time-dependent two-level propagation model, respectively. Self-phase modulation and stimulated Raman scattering are found to limit the usable data format space. In operational regimes free from nonlinear effects, dynamic gain effects such as the variation in the output pulse energy and square-pulse distortion are quantified. Both are found to primarily depend on the symbol duration and can be as large as 28% and 21%, respectively. (C) 2014 Optical Society of America
C1 [Yao, Haomin; Marciante, John R.] Univ Rochester, Inst Opt, Rochester, NY 14627 USA.
   [Wright, Malcolm W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Yao, HM (reprint author), Univ Rochester, Inst Opt, Rochester, NY 14627 USA.
EM hayao@optics.rochester.edu
RI Chen, Ru/A-5105-2015
FU NASA/JPL [1440052]; National Aeronautics and Space Administration
FX H. Yao and J. R. Marciante were supported in part by NASA/JPL under
   Subcontract No. 1440052. The work of M. W. Wright was carried out at the
   Jet Propulsion Laboratory, California Institute of Technology under
   contract with the National Aeronautics and Space Administration. H. Yao
   thanks Jordan Leidner and Dr. George Gehring for helpful technical
   discussions.
NR 19
TC 0
Z9 0
U1 0
U2 4
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD SEP 20
PY 2014
VL 53
IS 27
BP 6155
EP 6161
DI 10.1364/AO.53.006155
PG 7
WC Optics
SC Optics
GA AP3TP
UT WOS:000342000900033
PM 25322091
ER

PT J
AU Ackermann, M
   Albert, A
   Atwood, WB
   Baldini, L
   Ballet, J
   Barbiellini, G
   Bastieri, D
   Bellazzini, R
   Bissaldi, E
   Blandford, RD
   Bloom, ED
   Bottacini, E
   Brandt, TJ
   Bregeon, J
   Bruel, P
   Buehler, R
   Buson, S
   Caliandro, GA
   Cameron, RA
   Caragiulo, M
   Caraveo, PA
   Cavazzuti, E
   Cecchi, C
   Charles, E
   Chekhtman, A
   Chiang, J
   Chiaro, G
   Ciprini, S
   Claus, R
   Cohen-Tanugi, J
   Conrad, J
   Cutini, S
   D'Ammando, F
   de Angelis, A
   de Palma, F
   Dermer, CD
   Digel, SW
   Di Venere, L
   Silva, EDE
   Drell, PS
   Favuzzi, C
   Ferrara, EC
   Focke, WB
   Franckowiak, A
   Fukazawa, Y
   Funk, S
   Fusco, P
   Gargano, F
   Gasparrini, D
   Germani, S
   Giglietto, N
   Giordano, F
   Giroletti, M
   Godfrey, G
   Gomez-Vargas, GA
   Grenier, IA
   Guiriec, S
   Hadasch, D
   Harding, AK
   Hays, E
   Hewitt, JW
   Hou, X
   Jogler, T
   Johannesson, G
   Johnson, AS
   Johnson, WN
   Kamae, T
   Kataoka, J
   Knodlseder, J
   Kocevski, D
   Kuss, M
   Larsson, S
   Latronico, L
   Longo, F
   Loparco, F
   Lovellette, MN
   Lubrano, P
   Malyshev, D
   Manfreda, A
   Massaro, F
   Mayer, M
   Mazziotta, MN
   McEnery, JE
   Michelson, PF
   Mitthumsiri, W
   Mizuno, T
   Monzani, ME
   Morselli, A
   Moskalenko, IV
   Murgia, S
   Nemmen, R
   Nuss, E
   Ohsugi, T
   Omodei, N
   Orienti, M
   Orlando, E
   Ormes, JF
   Paneque, D
   Panetta, JH
   Perkins, JS
   Pesce-Rollins, M
   Petrosian, V
   Piron, F
   Pivato, G
   Raino, S
   Rando, R
   Razzano, M
   Razzaque, S
   Reimer, A
   Reimer, O
   Sanchez-Conde, M
   Schaal, M
   Schulz, A
   Sgro, C
   Siskind, EJ
   Spandre, G
   Spinelli, P
   Stawarz, L
   Strong, AW
   Suson, DJ
   Tahara, M
   Takahashi, H
   Thayer, JB
   Tibaldo, L
   Tinivella, M
   Torres, DF
   Tosti, G
   Troja, E
   Uchiyama, Y
   Vianello, G
   Werner, M
   Winer, BL
   Wood, KS
   Wood, M
   Zaharijas, G
AF Ackermann, M.
   Albert, A.
   Atwood, W. B.
   Baldini, L.
   Ballet, J.
   Barbiellini, G.
   Bastieri, D.
   Bellazzini, R.
   Bissaldi, E.
   Blandford, R. D.
   Bloom, E. D.
   Bottacini, E.
   Brandt, T. J.
   Bregeon, J.
   Bruel, P.
   Buehler, R.
   Buson, S.
   Caliandro, G. A.
   Cameron, R. A.
   Caragiulo, M.
   Caraveo, P. A.
   Cavazzuti, E.
   Cecchi, C.
   Charles, E.
   Chekhtman, A.
   Chiang, J.
   Chiaro, G.
   Ciprini, S.
   Claus, R.
   Cohen-Tanugi, J.
   Conrad, J.
   Cutini, S.
   D'Ammando, F.
   de Angelis, A.
   de Palma, F.
   Dermer, C. D.
   Digel, S. W.
   Di Venere, L.
   do Couto e Silva, E.
   Drell, P. S.
   Favuzzi, C.
   Ferrara, E. C.
   Focke, W. B.
   Franckowiak, A.
   Fukazawa, Y.
   Funk, S.
   Fusco, P.
   Gargano, F.
   Gasparrini, D.
   Germani, S.
   Giglietto, N.
   Giordano, F.
   Giroletti, M.
   Godfrey, G.
   Gomez-Vargas, G. A.
   Grenier, I. A.
   Guiriec, S.
   Hadasch, D.
   Harding, A. K.
   Hays, E.
   Hewitt, J. W.
   Hou, X.
   Jogler, T.
   Johannesson, G.
   Johnson, A. S.
   Johnson, W. N.
   Kamae, T.
   Kataoka, J.
   Knoedlseder, J.
   Kocevski, D.
   Kuss, M.
   Larsson, S.
   Latronico, L.
   Longo, F.
   Loparco, F.
   Lovellette, M. N.
   Lubrano, P.
   Malyshev, D.
   Manfreda, A.
   Massaro, F.
   Mayer, M.
   Mazziotta, M. N.
   McEnery, J. E.
   Michelson, P. F.
   Mitthumsiri, W.
   Mizuno, T.
   Monzani, M. E.
   Morselli, A.
   Moskalenko, I. V.
   Murgia, S.
   Nemmen, R.
   Nuss, E.
   Ohsugi, T.
   Omodei, N.
   Orienti, M.
   Orlando, E.
   Ormes, J. F.
   Paneque, D.
   Panetta, J. H.
   Perkins, J. S.
   Pesce-Rollins, M.
   Petrosian, V.
   Piron, F.
   Pivato, G.
   Raino, S.
   Rando, R.
   Razzano, M.
   Razzaque, S.
   Reimer, A.
   Reimer, O.
   Sanchez-Conde, M.
   Schaal, M.
   Schulz, A.
   Sgro, C.
   Siskind, E. J.
   Spandre, G.
   Spinelli, P.
   Stawarz, Lukasz
   Strong, A. W.
   Suson, D. J.
   Tahara, M.
   Takahashi, H.
   Thayer, J. B.
   Tibaldo, L.
   Tinivella, M.
   Torres, D. F.
   Tosti, G.
   Troja, E.
   Uchiyama, Y.
   Vianello, G.
   Werner, M.
   Winer, B. L.
   Wood, K. S.
   Wood, M.
   Zaharijas, G.
TI THE SPECTRUM AND MORPHOLOGY OF THE FERMI BUBBLES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astroparticle physics; cosmic rays; Galaxy: general; Galaxy: halo; gamma
   rays: diffuse background; methods: data analysis
ID LARGE-AREA TELESCOPE; COSMIC-RAY PROPAGATION; CONTINUUM GAMMA-RAYS; P-P
   INTERACTION; MILKY-WAY; X-RAY; ASTRONOMICAL ENVIRONMENTS;
   INTERSTELLAR-MEDIUM; COMPTON-SCATTERING; HELIUM SPECTRA
AB The Fermi bubbles are two large structures in the gamma-ray sky extending to 55 degrees above and below the Galactic center. We analyze 50 months of Fermi Large Area Telescope data between 100MeV and 500 GeV above 10 degrees in Galactic latitude to derive the spectrum and morphology of the Fermi bubbles. We thoroughly explore the systematic uncertainties that arise when modeling the Galactic diffuse emission through two separate approaches. The gamma-ray spectrum is well described by either a log parabola or a power law with an exponential cutoff. We exclude a simple power law with more than 7 sigma significance. The power law with an exponential cutoff has an index of 1.9 +/- 0.2 and a cutoff energy of 110 +/- 50 GeV. We find that the gamma-ray luminosity of the bubbles is 4.4(-0.9)(+2.4) x 10(37) erg s(-1). We confirm a significant enhancement of gamma-ray emission in the southeastern part of the bubbles, but we do not find significant evidence for a jet. No significant variation of the spectrum across the bubbles is detected. The width of the boundary of the bubbles is estimated to be 3.4(-2.6)(+3.7) deg. Both inverse Compton (IC) models and hadronic models including IC emission from secondary leptons fit the gamma-ray data well. In the IC scenario, synchrotron emission from the same population of electrons can also explain the WMAP and Planck microwave haze with a magnetic field between 5 and 20 mu G.
C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] DESY, D-15738 Zeuthen, Germany.
   [Albert, A.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Funk, S.; Godfrey, G.; Jogler, T.; Johnson, A. S.; Kamae, T.; Malyshev, D.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Petrosian, V.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Thayer, J. B.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
   [Albert, A.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Funk, S.; Godfrey, G.; Jogler, T.; Johnson, A. S.; Kamae, T.; Malyshev, D.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Petrosian, V.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Tibaldo, L.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
   [Atwood, W. B.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
   [Atwood, W. B.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Baldini, L.; Bellazzini, R.; Kuss, M.; Manfreda, A.; Pesce-Rollins, M.; Sgro, C.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
   [Ballet, J.] Univ Paris Diderot, CNRS, CEA Saclay, CEA IRFU,Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France.
   [Barbiellini, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
   [Barbiellini, G.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
   [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
   [Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
   [Bissaldi, E.; Zaharijas, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
   [Bissaldi, E.; Zaharijas, G.] Univ Trieste, I-34127 Trieste, Italy.
   [Brandt, T. J.; Ferrara, E. C.; Harding, A. K.; Hays, E.; Kocevski, D.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Bregeon, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, IN2P3, CNRS, Lab Univ & 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.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
   [Caraveo, P. A.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
   [Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00133 Rome, Italy.
   [Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
   [Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
   [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
   [Ciprini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Roma, Italy.
   [Conrad, J.; Larsson, S.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.
   [Conrad, J.; Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
   [Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden.
   [D'Ammando, F.] INAF, Ist Radioastron, I-40129 Bologna, Italy.
   [D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
   [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
   [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
   [Dermer, C. D.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] Div Space Sci, Naval Res Lab, Washington, DC 20375 USA.
   [Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
   [Fukazawa, Y.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
   [Gomez-Vargas, G. A.; Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
   [Gomez-Vargas, G. A.] Pontificia Univ Catolica Chile, Dipartimento Fis, Santiago, Chile.
   [Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
   [Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
   [Hewitt, J. W.; Nemmen, R.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
   [Hewitt, J. W.; Nemmen, R.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
   [Hewitt, J. W.; Nemmen, R.] CRESST, Greenbelt, MD 20771 USA.
   [Hewitt, J. W.; Nemmen, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Hou, X.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
   [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
   [Kataoka, J.; Tahara, M.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
   [Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France.
   [Knoedlseder, J.] Univ Toulouse, IRAP, UPS OMP, GAHEC, Toulouse, France.
   [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
   [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
   [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.
   [McEnery, J. E.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
   [McEnery, J. E.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Mitthumsiri, W.] Mahidol Univ, Fac Sci, Dept Phys, Bangkok 10400, Thailand.
   [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
   [Murgia, S.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA.
   [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
   [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
   [Razzaque, S.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa.
   [Schaal, M.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
   [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
   [Stawarz, Lukasz] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
   [Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
   [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.
   [Torres, D. F.] CSIC, IEEE, Inst Ciencies Espai, Barcelona 08193, Spain.
   [Torres, D. F.] ICREA, Barcelona, Spain.
   [Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA.
   [Zaharijas, G.] Abdus Salam Int Ctr Theoret Phys, I-34151 Trieste, Italy.
RP Ackermann, M (reprint author), DESY, D-15738 Zeuthen, Germany.
EM afrancko@slac.stanford.edu; malyshev@stanford.edu; vahep@stanford.edu
RI Massaro, Francesco/L-9102-2016; Torres, Diego/O-9422-2016; Orlando,
   E/R-5594-2016; Di Venere, Leonardo/C-7619-2017; Morselli,
   Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Reimer, Olaf/A-3117-2013;
   Funk, Stefan/B-7629-2015; Gomez-Vargas, German/C-7138-2015; Johannesson,
   Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario
   /O-8867-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012;
   Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Bissaldi,
   Elisabetta/K-7911-2016; 
OI Massaro, Francesco/0000-0002-1704-9850; Torres,
   Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X;
   Giordano, Francesco/0000-0002-8651-2394; Caraveo,
   Patrizia/0000-0003-2478-8018; SPINELLI, Paolo/0000-0001-6688-8864;
   Bastieri, Denis/0000-0002-6954-8862; orienti,
   monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852;
   Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385;
   Funk, Stefan/0000-0002-2012-0080; Johannesson,
   Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673;
   Mazziotta, Mario /0000-0001-9325-4672; Gargano,
   Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888;
   Moskalenko, Igor/0000-0001-6141-458X; Bissaldi,
   Elisabetta/0000-0001-9935-8106; Gasparrini, Dario/0000-0002-5064-9495;
   Baldini, Luca/0000-0002-9785-7726
FU Italian Ministry of Education, University and Research (MIUR)
   [FIRB-2012-RBFR12PM1F]
FX Funded by contract FIRB-2012-RBFR12PM1F from the Italian Ministry of
   Education, University and Research (MIUR).
NR 66
TC 70
Z9 72
U1 1
U2 23
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 2014
VL 793
IS 1
AR 64
DI 10.1088/0004-637X/793/1/64
PG 34
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4IW
UT WOS:000341301700064
ER

PT J
AU Anderson, CN
   Meier, DS
   Ott, J
   Hughes, A
   Wong, T
   Henkel, C
   Chen, R
   Indebetouw, R
   Looney, L
   Muller, E
   Pineda, JL
   Seale, J
AF Anderson, Crystal N.
   Meier, David S.
   Ott, Juergen
   Hughes, Annie
   Wong, Tony
   Henkel, Christian
   Chen, Rosie
   Indebetouw, Remy
   Looney, Leslie
   Muller, Erik
   Pineda, Jorge L.
   Seale, Jonathan
TI FROM GAS TO STARS IN ENERGETIC ENVIRONMENTS: DENSE GAS CLUMPS IN THE 30
   DORADUS REGION WITHIN THE LARGE MAGELLANIC CLOUD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: abundances; galaxies: individual (Large Magellanic Clouds);
   ISM: molecules
ID GIANT MOLECULAR CLOUDS; INFRARED GALAXIES; CO SURVEY; CORES; ABUNDANCES;
   STARBURST; EMISSION; CLUSTERS; HCO+; HCN
AB We present parsec-scale interferometric maps of HCN(1-0) and HCO+(1-0) emission from dense gas in the star-forming region 30 Doradus, obtained using the Australia Telescope Compact Array. This extreme star-forming region, located in the Large Magellanic Cloud (LMC), is characterized by a very intense ultraviolet ionizing radiation field and sub-solar metallicity, both of which are expected to impact molecular cloud structure. We detect 13 bright, dense clumps within the 30 Doradus-10 giant molecular cloud. Some of the clumps are aligned along a filamentary structure with a characteristic spacing that is consistent with formation via varicose fluid instability. Our analysis shows that the filament is gravitationally unstable and collapsing to form stars. There is a good correlation between HCO+ emission in the filament and signatures of recent star formation activity including H2O masers and young stellar objects (YSOs). YSOs seem to continue along the same direction of the filament toward the massive compact star cluster R136 in the southwest. We present detailed comparisons of clump properties (masses, linewidths, and sizes) in 30Dor-10 to those in other star forming regions of the LMC (N159, N113, N105, and N44). Our analysis shows that the 30Dor-10 clumps have similar masses but wider linewidths and similar HCN/HCO+ (1-0) line ratios as clumps detected in other LMC star-forming regions. Our results suggest that the dense molecular gas clumps in the interior of 30Dor-10 are well shielded against the intense ionizing field that is present in the 30Doradus region.
C1 [Anderson, Crystal N.; Meier, David S.; Ott, Juergen] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
   [Meier, David S.; Ott, Juergen] Natl Radio Astron Observ, Socorro, NM 87801 USA.
   [Hughes, Annie] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Wong, Tony; Looney, Leslie] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
   [Henkel, Christian; Chen, Rosie] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
   [Henkel, Christian] King Abdulaziz Univ, Dept Astron, Jeddah 21589, Saudi Arabia.
   [Indebetouw, Remy] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
   [Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
   [Muller, Erik] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
   [Pineda, Jorge L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Seale, Jonathan] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Anderson, CN (reprint author), New Mexico Inst Min & Technol, Dept Phys, 801 Leroy Pl, Socorro, NM 87801 USA.
FU NSF [AST-1009620]
FX Part of this research was conducted at the Jet Propulsion Laboratory,
   California Institute of Technology under contract with the National
   Aeronautics and Space Administration. Part of this project was funded by
   NSF Grant AST-1009620 to D.S.M. This research has made use of the SIMBAD
   database, operated at CDS, Strasbourg, France. This paper makes use of
   the following ALMA data: ADS/JAO. ALMA #2011.0.00471. S. ALMA is a
   partnership of ESO (representing its member states), NSF (USA) and NINS
   (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in
   cooperation with the Republic of Chile. The Joint ALMA Observatory is
   operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy
   Observatory is a facility of the National Science Foundation operated
   under cooperative agreement by Associated Universities, Inc.
NR 42
TC 5
Z9 5
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 20
PY 2014
VL 793
IS 1
AR 37
DI 10.1088/0004-637X/793/1/37
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4IW
UT WOS:000341301700037
ER

PT J
AU Ansdell, M
   Meech, KJ
   Hainaut, O
   Buie, MW
   Kaluna, H
   Bauer, J
   Dundon, L
AF Ansdell, Megan
   Meech, Karen J.
   Hainaut, Olivier
   Buie, Marc W.
   Kaluna, Heather
   Bauer, James
   Dundon, Luke
TI REFINED ROTATIONAL PERIOD, POLE SOLUTION, AND SHAPE MODEL FOR (3200)
   PHAETHON
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids: individual (3200 Phaethon); techniques:
   photometric
ID ASTEROID LIGHTCURVE INVERSION; NEAR-EARTH ASTEROIDS; OPTIMIZATION
   METHODS; STREAM; OBJECTS; PARENT
AB (3200) Phaethon exhibits both comet-and asteroid-like properties, suggesting it could be a rare transitional object such as a dormant comet or previously volatile-rich asteroid. This justifies detailed study of (3200) Phaethon's physical properties as a better understanding of asteroid-comet transition objects can provide insight into minor body evolution. We therefore acquired time series photometry of (3200) Phaethon over 15 nights from 1994 to 2013, primarily using the Tektronix 2048 x 2048 pixel CCD on the University of Hawaii 2.2 m telescope. We utilized light curve inversion to (1) refine (3200) Phaethon's rotational period to P = 3.6032 +/- 0.0008 hr; (2) estimate a rotational pole orientation of lambda = +85 degrees +/- 13 degrees and beta = -20 degrees +/- 10 degrees.; and (3) derive a shape model. We also used our extensive light curve data set to estimate the slope parameter of (3200) Phaethon's phase curve as G similar to 0.06, consistent with C-type asteroids. We discuss how this highly oblique pole orientation with a negative ecliptic latitude supports previous evidence for (3200) Phaethon's origin in the inner main asteroid belt as well as the potential for deeply buried volatiles fueling impulsive yet rare cometary outbursts.
C1 [Ansdell, Megan; Meech, Karen J.; Kaluna, Heather] NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
   [Ansdell, Megan; Meech, Karen J.; Kaluna, Heather] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
   [Hainaut, Olivier] European So Observ, D-85748 Garching, Germany.
   [Buie, Marc W.] Southwest Res Inst, Boulder, CO 80302 USA.
   [Bauer, James] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Dundon, Luke] US Navy, Washington, DC 20350 USA.
RP Ansdell, M (reprint author), NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
EM mansdell@ifa.hawaii.edu
OI Ansdell, Megan/0000-0003-4142-9842
FU National Aeronautics and Space Administration through the NASA
   Astrobiology Institute [NNA04CC08A]; NASA [NAGW 5015, NAG5-4495,
   NNX07A044G, NNX13A151G, NNX07AF79G]
FX We thank the referee for the very detailed review of this work, which
   greatly improved the paper. We are extremely grateful to the telescope
   staff of UH88 and Lowell Observatory, without whom this work would not
   have been possible. A special thanks to Michael Belton for his
   insightful feedback on short notice. We also thank Josef Durech and his
   collaborators, who kindly provided the MATLAB code used to generate the
   shape model visualization. This work was supported by the National
   Aeronautics and Space Administration through the NASA Astrobiology
   Institute under Cooperative Agreement No. NNA04CC08A issued through the
   Office of Space Science, by NASA grant Nos. NAGW 5015, NAG5-4495,
   NNX07A044G, NNX13A151G, and NNX07AF79G. Image processing was done in
   part using the IRAF software. IRAF is distributed by the National
   Optical Astronomy Observatories, which is operated by the Association of
   Universities for Research in Astronomy, Inc. (AURA) under cooperative
   agreement with the National Science Foundation.
NR 38
TC 2
Z9 3
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2014
VL 793
IS 1
AR 50
DI 10.1088/0004-637X/793/1/50
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4IW
UT WOS:000341301700050
ER

PT J
AU Arcavi, I
   Gal-Yam, A
   Sullivan, M
   Pan, YC
   Cenko, SB
   Horesh, A
   Ofek, EO
   De Cia, A
   Yan, L
   Yang, CW
   Howell, DA
   Tal, D
   Kulkarni, SR
   Tendulkar, SP
   Tang, SM
   Xu, D
   Sternberg, A
   Cohen, JG
   Bloom, JS
   Nugent, PE
   Kasliwal, MM
   Perley, DA
   Quimby, RM
   Miller, AA
   Theissen, CA
   Laher, RR
AF Arcavi, Iair
   Gal-Yam, Avishay
   Sullivan, Mark
   Pan, Yen-Chen
   Cenko, S. Bradley
   Horesh, Assaf
   Ofek, Eran O.
   De Cia, Annalisa
   Yan, Lin
   Yang, Chen-Wei
   Howell, D. A.
   Tal, David
   Kulkarni, Shrinivas R.
   Tendulkar, Shriharsh P.
   Tang, Sumin
   Xu, Dong
   Sternberg, Assaf
   Cohen, Judith G.
   Bloom, Joshua S.
   Nugent, Peter E.
   Kasliwal, Mansi M.
   Perley, Daniel A.
   Quimby, Robert M.
   Miller, Adam A.
   Theissen, Christopher A.
   Laher, Russ R.
TI A CONTINUUM OF H- TO He-RICH TIDAL DISRUPTION CANDIDATES WITH A
   PREFERENCE FOR E plus A GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; galaxies: nuclei; quasars: supermassive
   black holes
ID DIGITAL SKY SURVEY; SUPERMASSIVE BLACK-HOLE; STELLAR POPULATION
   SYNTHESIS; ACTIVE GALACTIC NUCLEI; 1ST SPECTROSCOPIC DATA; STAR-FORMING
   GALAXIES; X-RAY OUTBURSTS; HIGH-REDSHIFT; CHANDRA OBSERVATIONS; SPECTRAL
   EVOLUTION
AB We present the results of a Palomar Transient Factory (PTF) archival search for blue transients that lie in the magnitude range between "normal" core-collapse and superluminous supernovae (i.e., with -21 <= M-R ((peak)) <= -19). Of the six events found after excluding all interacting Type IIn and Ia-CSM supernovae, three (PTF09ge, 09axc, and 09djl) are coincident with the centers of their hosts, one (10iam) is offset from the center, and a precise offset cannot be determined for two (10nuj and 11glr). All the central events have similar rise times to the He-rich tidal disruption candidate PS1-10jh, and the event with the best-sampled light curve also has similar colors and power-law decay. Spectroscopically, PTF09ge is He-rich, while PTF09axc and 09djl display broad hydrogen features around peak magnitude. All three central events are in low star formation hosts, two of which are E+A galaxies. Our spectrum of the host of PS1-10jh displays similar properties. PTF10iam, the one offset event, is different photometrically and spectroscopically from the central events, and its host displays a higher star formation rate. Finding no obvious evidence for ongoing galactic nuclei activity or recent star formation, we conclude that the three central transients likely arise from the tidal disruption of a star by a supermassive black hole. We compare the spectra of these events to tidal disruption candidates from the literature and find that all of these objects can be unified on a continuous scale of spectral properties. The accumulated evidence of this expanded sample strongly supports a tidal disruption origin for this class of nuclear transients.
C1 [Arcavi, Iair; Gal-Yam, Avishay; Pan, Yen-Chen; Cenko, S. Bradley; Horesh, Assaf; Tal, David] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
   [Arcavi, Iair; Howell, D. A.] Las Cumbres Observ Global Telescope, Goleta, CA 93111 USA.
   [Arcavi, Iair] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
   [Sullivan, Mark] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
   [Pan, Yen-Chen] Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England.
   [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.
   [Yan, Lin; Yang, Chen-Wei] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
   [Yang, Chen-Wei] Univ Sci & Technol China, Chinese Acad Sci, Key Lab Res Galaxies & Cosmol, Hefei 230026, Anhui, Peoples R China.
   [Howell, D. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
   [Kulkarni, Shrinivas R.; Tendulkar, Shriharsh P.; Tang, Sumin; Cohen, Judith G.; Perley, Daniel A.; Miller, Adam A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
   [Xu, Dong] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark.
   [Sternberg, Assaf] Tech Univ Munich, Excellence Cluster Univ, D-85748 Garching, Germany.
   [Sternberg, Assaf] Max Planck Inst Astrophys, D-85748 Garching, Germany.
   [Bloom, Joshua S.; Nugent, Peter E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Bloom, Joshua S.; Nugent, Peter E.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
   [Kasliwal, Mansi M.] Carnegie Inst Sci, Pasadena, CA 91101 USA.
   [Quimby, Robert M.] Univ Tokyo, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan.
   [Miller, Adam A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Theissen, Christopher A.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
   [Laher, Russ R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Arcavi, I (reprint author), Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
EM iarcavi@lcogt.net
RI Horesh, Assaf/O-9873-2016; 
OI Horesh, Assaf/0000-0002-5936-1156; Sullivan, Mark/0000-0001-9053-4820;
   Arcavi, Iair/0000-0001-7090-4898; Theissen,
   Christopher/0000-0002-9807-5435; Gal-Yam, Avishay/0000-0002-3653-5598
FU Israeli Science Foundation; EU/FP7/ERC grant; BSF; GIF; Minerva;
   "Quantum Universe" I-Core program of the planning and budgeting
   committee; ISF; Kimmel Investigator award; Israeli Ministry of Science;
   I-CORE Program of the Planning and Budgeting Committee; Israel Science
   Foundation [1829/12]; Hubble Fellowship; Carnegie-Princeton Fellowship;
   NASA/Swift Guest Investigator [NNX09AQ66G, NNX10AF93G, NSF/AST-100991];
   NASA [HST-HF-51325.01]
FX A.G. and I.A. acknowledge support by the Israeli Science Foundation and
   an EU/FP7/ERC grant. A.G. further acknowledges grants from the BSF, GIF,
   and Minerva, as well as the "Quantum Universe" I-Core program of the
   planning and budgeting committee and the ISF, and a Kimmel Investigator
   award. E.O.O. is incumbent of the Arye Dissentshik career development
   chair and is grateful for support by a grant from the Israeli Ministry
   of Science and the I-CORE Program of the Planning and Budgeting
   Committee and The Israel Science Foundation (grant No. 1829/12). M.M.K.
   acknowledges generous support from the Hubble Fellowship and
   Carnegie-Princeton Fellowship. J.S.B. and his group were partially
   supported by NASA/Swift Guest Investigator grants NNX09AQ66G and
   NNX10AF93G, and NSF/AST-100991. A.A.M. acknowledges support for this
   work by NASA from a Hubble Fellowship grant HST-HF-51325.01.
NR 109
TC 67
Z9 67
U1 1
U2 11
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 2014
VL 793
IS 1
AR 38
DI 10.1088/0004-637X/793/1/38
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4IW
UT WOS:000341301700038
ER

PT J
AU Bolmont, E
   Raymond, SN
   von Paris, P
   Selsis, F
   Hersant, F
   Quintana, EV
   Barclay, T
AF Bolmont, Emeline
   Raymond, Sean N.
   von Paris, Philip
   Selsis, Franck
   Hersant, Franck
   Quintana, Elisa V.
   Barclay, Thomas
TI FORMATION, TIDAL EVOLUTION, AND HABITABILITY OF THE KEPLER-186 SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: numerical; planets and satellites: atmospheres; planets and
   satellites: dynamical evolution and stability; planets and satellites:
   formation; stars: individual (Kepler-186, KIC 8120608)
ID TERRESTRIAL PLANET FORMATION; MAIN-SEQUENCE STARS; HIGH-RESOLUTION
   SIMULATIONS; SHORT-PERIOD PLANETS; EARTH-SIZED PLANET; M-DWARF STARS;
   SUN-LIKE STAR; WATER DELIVERY; LOW-MASS; SUPER-EARTHS
AB The Kepler-186 system consists of five planets orbiting an early M dwarf. The planets have physical radii of 1.0-1.50 R-circle plus and orbital periods of 4-130 days. The 1.1 R-circle plus Kepler-186f with a period of 130 days is of particular interest. Its insolation of roughly 0.32 S-circle plus places it within the surface liquid water habitable zone (HZ). We present a multifaceted study of the Kepler-186 system, using two sets of parameters which are consistent with the data and also self-consistent. First, we show that the distribution of planet masses can be roughly reproduced if the planets were accreted from a high surface density disk presumably sculpted by an earlier phase of migration. However, our simulations predict the existence of one to two undetected planets between planets e and f. Next, we present a dynamical analysis of the system including the effect of tides. The timescale for tidal evolution is short enough that the four inner planets must have small obliquities and near-synchronous rotation rates. The tidal evolution of Kepler-186f is slow enough that its current spin state depends on a combination of its initial spin state, its dissipation rate, and the stellar age. Finally, we study the habitability of Kepler-186f with a one-dimensional climate model. The planet's surface temperature can be raised above 273 K with 0.5-5 bars of CO2, depending on the amount of N-2 present. Kepler-186f represents a case study of an Earth-sized planet in the cooler regions of the HZ of a cool star.
C1 [Bolmont, Emeline; Raymond, Sean N.; Selsis, Franck; Hersant, Franck] Univ Bordeaux, Lab Astrophys Bordeaux, UMR 5804, F-33270 Florac, France.
   [Bolmont, Emeline; Raymond, Sean N.; Selsis, Franck; Hersant, Franck] CNRS, Lab Astrophys Bordeaux, UMR 5804, F-33270 Floirac, France.
   [von Paris, Philip] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetenforsch, D-12489 Berlin, Germany.
   [Quintana, Elisa V.] SETI Inst, Mountain View, CA 94043 USA.
   [Quintana, Elisa V.; Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Barclay, Thomas] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
RP Bolmont, E (reprint author), Univ Bordeaux, Lab Astrophys Bordeaux, UMR 5804, F-33270 Florac, France.
EM bolmont@obs.u-bordeaux1.fr
FU Agence Nationale pour la Recherche [ANR-13-BS05-0003-02]; NASA
   [NNA13AA93A]; Helmholtz Association; French State in the frame of the
   "Investments for the future" Programme IdEx Bordeaux
   [ANR-10-IDEX-03-02]; European Research Council [209622: E3ARTHs]
FX S.N.R. and F.H. are grateful to the Agence Nationale pour la Recherche
   via grant ANR-13-BS05-0003-02 (project MOJO). S.N.R.'s contribution was
   performed as part of the NASA Astrobiology Institute's Virtual Planetary
   Laboratory Lead Team, supported by NASA under Cooperative Agreement No.
   NNA13AA93A.; This research has been partly supported by the Helmholtz
   Association through the research alliance "Planetary Evolution and
   Life." This study has received financial support from the French State
   in the frame of the "Investments for the future" Programme IdEx
   Bordeaux, reference ANR-10-IDEX-03-02.; F.S. acknowledges support from
   the European Research Council (Starting Grant 209622:
   E<INF>3</INF>ARTHs)
NR 138
TC 9
Z9 9
U1 4
U2 46
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 2014
VL 793
IS 1
AR 3
DI 10.1088/0004-637X/793/1/3
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4IW
UT WOS:000341301700003
ER

PT J
AU Cohen, CMS
   Mason, GM
   Mewaldt, RA
   Wiedenbeck, ME
AF Cohen, C. M. S.
   Mason, G. M.
   Mewaldt, R. A.
   Wiedenbeck, M. E.
TI THE LONGITUDINAL DEPENDENCE OF HEAVY-ION COMPOSITION IN THE 2013 APRIL
   11 SOLAR ENERGETIC PARTICLE EVENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; Sun: activity; Sun: coronal mass ejections
   (CMEs); Sun: particle emission
ID ISOTOPE SPECTROMETER; PEAK INTENSITIES; STEREO MISSION; HIGH-ENERGIES;
   ACE; ACCELERATION; VARIABILITY; ABUNDANCES; SPACECRAFT; TELESCOPE
AB On 2013 April 11 active region 11719 was centered just west of the central meridian; at 06:55 UT, it erupted with an M6.5 X-ray flare and a moderately fast (similar to 800 km s(-1)) coronal mass ejection. This solar activity resulted in the acceleration of energetic ions to produce a solar energetic particle (SEP) event that was subsequently observed in energetic protons by both ACE and the two STEREO spacecraft. Heavy ions at energies >= 10 MeV nucleon(-1) were well measured by SEP sensors on ACE and STEREO-B, allowing the longitudinal dependence of the event composition to be studied. Both spacecraft observed significant enhancements in the Fe/O ratio at 12-33 MeV nucleon(-1), with the STEREO-B abundance ratio (Fe/O = 0.69) being similar to that of the large, Fe-rich SEP events observed in solar cycle 23. The footpoint of the magnetic field line connected to the ACE spacecraft was longitudinally farther from the flare site (77 degrees versus 58 degrees), and the measured Fe/O ratio at ACE was 0.48, 44% lower than at STEREO-B but still enhanced by more than a factor of 3.5 over average SEP abundances. Only upper limits were obtained for the He-3/He-4 abundance ratio at both spacecraft. Low upper limits of 0.07% and 1% were obtained from the ACE sensors at 0.5-2 and 6.5-11.3 MeV nucleon(-1), respectively, whereas the STEREO-B sensor provided an upper limit of 4%. These characteristics of high, but longitudinally variable, Fe/O ratios and low He-3/He-4 ratios are not expected from either the direct flare contribution scenario or the remnant flare suprathermal material theory put forth to explain the Fe-rich SEP events of cycle 23.
C1 [Cohen, C. M. S.; Mewaldt, R. A.] CALTECH, Pasadena, CA 91125 USA.
   [Mason, G. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
   [Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Cohen, CMS (reprint author), CALTECH, Pasadena, CA 91125 USA.
FU NASA at Caltech; UC Berkeley under NASA [SA2715-26309, NAS5-03131T];
   NASA [NNX11A075G, NNX13AH66G, NNX13AR20G, 44A-1091698]; NSF [1156004];
   NSF SHINE [1156138]; UC Berkeley [SA4889-26309]
FX This work was supported by NASA at Caltech and JPL under subcontract
   SA2715-26309 from UC Berkeley under NASA contract NAS5-03131T, and by
   NASA grants NNX11A075G and NNX13AH66G. It was also supported by the NSF
   under the grant 1156004. Work at APL was supported by NASA grants
   NNX13AR20G and 44A-1091698, as well as NSF SHINE grant 1156138 and UC
   Berkeley subcontract SA4889-26309. We thank the NASA CDAW Data Center
   and the Catholic University of America and ESA's CACTus project for
   their CME catalogs. We also thank the Michigan State University National
   Superconducting Cyclotron Lab for accelerator time and staff assistance
   in calibrating the response of the ACE/SIS and STEREO/LET sensors to
   energetic ions and in testing the related onboard analysis processes.
NR 32
TC 11
Z9 11
U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2014
VL 793
IS 1
AR 35
DI 10.1088/0004-637X/793/1/35
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4IW
UT WOS:000341301700035
ER

PT J
AU Line, MR
   Fortney, JJ
   Marley, MS
   Sorahana, S
AF Line, Michael R.
   Fortney, Jonathan J.
   Marley, Mark S.
   Sorahana, Satoko
TI A DATA-DRIVEN APPROACH FOR RETRIEVING TEMPERATURES AND ABUNDANCES IN
   BROWN DWARF ATMOSPHERES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; methods: statistical; radiative transfer; stars:
   atmospheres; stars: individual (Gl 570D)
ID TO-OXYGEN RATIO; LOW MASS STARS; AKARI OBSERVATIONS; CARBON-MONOXIDE;
   GLIESE 229B; INFRARED SPECTROGRAPH; CHEMICAL-EQUILIBRIUM; EXTRASOLAR
   PLANETS; RADIATIVE-TRANSFER; MODEL ATMOSPHERES
AB Brown dwarf spectra contain a wealth of information about their molecular abundances, temperature structure, and gravity. We present a new data driven retrieval approach, previously used in planetary atmosphere studies, to extract the molecular abundances and temperature structure from brown dwarf spectra. The approach makes few a priori physical assumptions about the state of the atmosphere. The feasibility of the approach is first demonstrated on a synthetic brown dwarf spectrum. Given typical spectral resolutions, wavelength coverage, and noise, property precisions of tens of percent can be obtained for the molecular abundances and tens to hundreds of K on the temperature profile. The technique is then applied to the well-studied brown dwarf, Gl 570D. From this spectral retrieval, the spectroscopic radius is constrained to be 0.75-0.83 R-J, log(g) to be 5.13-5.46, and T-eff to be between 804 and 849 K. Estimates for the range of abundances and allowed temperature profiles are also derived. The results from our retrieval approach are in agreement with the self-consistent grid modeling results of Saumon et al. This new approach will allow us to address issues of compositional differences between brown dwarfs and possibly their formation environments, disequilibrium chemistry, and missing physics in current grid modeling approaches as well as a many other issues.
C1 [Line, Michael R.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Marley, Mark S.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Sorahana, Satoko] Nagoya Univ, Dept Phys, Nagoya, Aichi 4648602, Japan.
RP Line, MR (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
EM mrline@ucsc.edu
RI Marley, Mark/I-4704-2013; 
OI Marley, Mark/0000-0002-5251-2943
FU NSF [AST-1312545]; NASA Astrophysics Theory Program
FX We thank Didier Saumon and Caroline Morley for reading the manuscript
   and providing instructive comments. J.J.F. acknowledges NSF grant
   AST-1312545. M.S.M. acknowledges the support of the NASA Astrophysics
   Theory Program.
NR 63
TC 10
Z9 10
U1 1
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2014
VL 793
IS 1
AR 33
DI 10.1088/0004-637X/793/1/33
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4IW
UT WOS:000341301700033
ER

PT J
AU Puccetti, S
   Comastri, A
   Fiore, F
   Arevalo, P
   Risaliti, G
   Bauer, FE
   Brandt, WN
   Stern, D
   Harrison, FA
   Alexander, DM
   Boggs, SE
   Christensen, FE
   Craig, WW
   Gandhi, P
   Hailey, CJ
   Koss, MJ
   Lansbury, GB
   Luo, B
   Madejski, GM
   Matt, G
   Walton, DJ
   Zhang, W
AF Puccetti, Simonetta
   Comastri, Andrea
   Fiore, Fabrizio
   Arevalo, Patricia
   Risaliti, Guido
   Bauer, Franz E.
   Brandt, William N.
   Stern, Daniel
   Harrison, Fiona A.
   Alexander, David M.
   Boggs, Steve E.
   Christensen, Finn E.
   Craig, William W.
   Gandhi, Poshak
   Hailey, Charles J.
   Koss, Michael J.
   Lansbury, George B.
   Luo, Bin
   Madejski, Greg M.
   Matt, Giorgio
   Walton, Dominic J.
   Zhang, Will
TI THE VARIABLE HARD X-RAY EMISSION OF NGC 4945 AS OBSERVED BY NUSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 4945); X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; EXTRAGALACTIC DISTANCE DATABASE; XMM-NEWTON;
   GALAXY NGC-4945; EDDINGTON RATIO; SPECTRUM; CHANDRA; SPECTROSCOPY; LINE;
   AGN
AB We present a broadband (similar to 0.5-79 keV) spectral and temporal analysis of multiple NuSTAR observations combined with archival Suzaku and Chandra data of NGC 4945, the brightest extragalactic source at 100 keV. We observe hard X-ray (>10 keV) flux and spectral variability, with flux variations of a factor of two on timescales of 20 ks. A variable primary continuum dominates the high-energy spectrum (>10 keV) in all states, while the reflected/scattered flux that dominates at E < 10 keV stays approximately constant. From modeling the complex reflection/transmission spectrum, we derive a Compton depth along the line of sight of tau(Thomson) similar to 2.9, and a global covering factor for the circumnuclear gas of similar to 0.15. This agrees with the constraints derived from the high-energy variability, which implies that most of the high-energy flux is transmitted rather than Compton-scattered. This demonstrates the effectiveness of spectral analysis at constraining the geometric properties of the circumnuclear gas, and validates similar methods used for analyzing the spectra of other bright, Compton-thick active galactic nuclei (AGNs). The lower limits on the e-folding energy are between 200 and 300 keV, consistent with previous BeppoSAX, Suzaku, and Swift Burst Alert Telescope observations. The accretion rate, estimated from the X-ray luminosity and assuming a bolometric correction typical of type 2 AGN, is in the range similar to 0.1-0.3 lambda(Edd) depending on the flux state. The substantial observed X-ray luminosity variability of NGC 4945 implies that large errors can arise from using single-epoch X-ray data to derive L/L-Edd values for obscured AGNs.
C1 [Puccetti, Simonetta] ASDC ASI, I-00133 Rome, Italy.
   [Puccetti, Simonetta; Fiore, Fabrizio] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
   [Comastri, Andrea] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
   [Arevalo, Patricia; Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile.
   [Risaliti, Guido] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
   [Risaliti, Guido] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA.
   [Brandt, William N.; Luo, Bin] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
   [Brandt, William N.; Luo, Bin] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
   [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Harrison, Fiona A.; Walton, Dominic J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
   [Alexander, David M.; Gandhi, Poshak; Lansbury, George B.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
   [Boggs, Steve E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
   [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
   [Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Koss, Michael J.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland.
   [Madejski, Greg M.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
   [Matt, Giorgio] Univ Roma Tre, Dipartimento Matemat Fis, I-00146 Rome, Italy.
   [Zhang, Will] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Puccetti, S (reprint author), ASDC ASI, Via Politecnico, I-00133 Rome, Italy.
RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt,
   William/N-2844-2015; XRAY, SUZAKU/A-1808-2009; Comastri,
   Andrea/O-9543-2015; 
OI Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581;
   Brandt, William/0000-0002-0167-2453; Comastri,
   Andrea/0000-0003-3451-9970; Risaliti, Guido/0000-0002-3556-977X;
   Puccetti, Simonetta/0000-0002-2734-7835; Fiore,
   Fabrizio/0000-0002-4031-4157
FU NASA [NNG08FD60C, GO3-14109X]; National Aeronautics and Space
   Administration; ASI/INAF [I/037/12/0-011/13]; STFC [ST/J003697/1,
   ST/K501979/1, ST/I001573/1]; Leverhulme Trust; Fondecyt [11100449];
   Anillo [ACT1101]; Swiss National Science Foundation [PP00P2_138979/1];
   California Institute of Technology NuSTAR [44A-1092750]; NASA ADP
   [NNX10AC99G]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [ACT1101, FONDECYT
   1101024]; "Millennium Institute of Astrophysics (MAS)" of Iniciativa
   Cientifica Milenio del Ministerio de Economia, Fomento y Turismo
   [IC120009]
FX This work was supported under NASA Contract 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). S.P., A.C., F.F., and G.M. acknowledge support from
   the ASI/INAF grant I/037/12/0-011/13. A.C. acknowledges the Caltech
   Kingsley visitor program. P.G. acknowledges support from STFC (grant
   reference ST/J003697/1). G.B.L. acknowledges support from STFC (grant
   reference ST/K501979/1). D.M.A. acknowledges support from STFC (grant
   reference ST/I001573/1) and from the Leverhulme Trust. P.A. acknowledges
   financial support from Fondecyt grant 11100449 and Anillo ACT1101. G.R.
   acknowledges financial support from grant NASA GO3-14109X. M.K.
   gratefully acknowledges support from Swiss National Science Foundation
   Grant PP00P2_138979/1. W.N.B. and B.L. acknowledge support from
   California Institute of Technology NuSTAR subcontract 44A-1092750 and
   NASA ADP Grant NNX10AC99G. F.E.B. acknowledges support from Basal-CATA
   PFB-06/2007, CONICYT-Chile (grants FONDECYT 1101024 and "EMBIGGEN"
   Anillo ACT1101), and Project IC120009 "Millennium Institute of
   Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de
   Economia, Fomento y Turismo. S.P. is grateful to Tahir Yaqoob for useful
   discussions on the MYTORUS model.
NR 59
TC 21
Z9 21
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 SEP 20
PY 2014
VL 793
IS 1
AR 26
DI 10.1088/0004-637X/793/1/26
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4IW
UT WOS:000341301700026
ER

PT J
AU Remya, B
   Tsurutani, BT
   Reddy, RV
   Lakhina, GS
   Falkowski, BJ
   Echer, E
   Glassmeier, KH
AF Remya, B.
   Tsurutani, B. T.
   Reddy, R. V.
   Lakhina, G. S.
   Falkowski, B. J.
   Echer, E.
   Glassmeier, K. -H.
TI LARGE-AMPLITUDE, CIRCULARLY POLARIZED, COMPRESSIVE, OBLIQUELY
   PROPAGATING ELECTROMAGNETIC PROTON CYCLOTRON WAVES THROUGHOUT THE
   EARTH'S MAGNETOSHEATH: LOW PLASMA beta CONDITIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instabilities; methods: data analysis; planets and satellites:
   individual (Earth, Cassini, WIND); planets and satellites: magnetic
   fields; polarization
ID MIRROR MODE WAVES; PITCH-ANGLE SCATTERING; COMET GIACOBINI-ZINNER;
   EQUATOR-S; SWING-BY; ANISOTROPY INSTABILITIES; ELECTRON-SCATTERING;
   GIOTTO OBSERVATIONS; DEPLETION LAYER; LION ROARS
AB During 1999 August 18, both Cassini and WIND were in the Earth's magnetosheath and detected transverse electromagnetic waves instead of the more typical mirror-mode emissions. The Cassini wave amplitudes were as large as similar to 14 nT (peak to peak) in a similar to 55 nT ambient magnetic field B-0. A new method of analysis is applied to study these waves. The general wave characteristics found were as follows. They were left-hand polarized and had frequencies in the spacecraft frame (f(scf)) below the proton cyclotron frequency (f(p)). Waves that were either right-hand polarized or had f(scf) > f(p) are shown to be consistent with Doppler-shifted left-hand waves with frequencies in the plasma frame f(pf) < f(p). Thus, almost all waves studied are consistent with their being electromagnetic proton cyclotron waves. Most of the waves (similar to 55%) were found to be propagating along B0 (theta(kB0) < 30 degrees), as expected from theory. However, a significant fraction of the waves were found to be propagating oblique to B0. These waves were also circularly polarized. This feature and the compressive ([B-max - B-min]/B-max, where B-max and B-min are the maximum and minimum field magnitudes) nature (ranging from 0.27 to 1.0) of the waves are noted but not well understood at this time. The proton cyclotron waves were shown to be quasi-coherent, theoretically allowing for rapid pitch-angle transport of resonant protons. Because Cassini traversed the entire subsolar magnetosheath and WIND was in the dusk-side flank of the magnetosheath, it is surmised that the entire region was filled with these waves. In agreement with past theory, it was the exceptionally low plasma beta (0.35) that led to the dominance of the proton cyclotron wave generation during this interval. A high-speed solar wind stream (< V-sw > = 598 km s(-1)) was the source of this low-beta plasma.
C1 [Remya, B.; Reddy, R. V.; Lakhina, G. S.] Indian Inst Geomagnetism, Navi Mumbai, Maharashtra, India.
   [Tsurutani, B. T.; Falkowski, B. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Echer, E.] Inst Nacl Pesquisas Espaciais, Sao Jose Dos Campos, SP, Brazil.
   [Glassmeier, K. -H.] IGEP, D-38106 Braunschweig, Germany.
RP Remya, B (reprint author), Indian Inst Geomagnetism, Kalamboli Highway, Navi Mumbai, Maharashtra, India.
EM remyaphysics@gmail.com
OI Remya, Bhanu/0000-0001-8356-8942
FU Indian Institute of Geomagnetism, Navi Mumbai, India; Jet Propulsion
   Laboratory, California Institute of Technology under NASA; National
   Academy of Sciences, India (NASI); CNPQ agency [301233/2011-0]; FAPESP
   agency [2012/06673-4]; German Bundesministerium fuer Wirtschaft und
   Technologie; Deutsches Zentrum fuer Luft-und Raumfahrt [50QP1001]
FX B. Remya thanks the Indian Institute of Geomagnetism, Navi Mumbai,
   India, for providing her with a Senior Research Fellowship and
   subsequently a Research Associateship to carry out this research work.
   Portions of this research were performed at the 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.
   E.E. acknowledges CNPQ agency contract 301233/2011-0 and FAPESP agency
   contract 2012/06673-4 for support for this work. The work of K.H.G. was
   financially supported by the German Bundesministerium fuer Wirtschaft
   und Technologie and the Deutsches Zentrum fuer Luft-und Raumfahrt under
   contract 50QP1001.
NR 75
TC 3
Z9 3
U1 2
U2 9
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 2014
VL 793
IS 1
AR 6
DI 10.1088/0004-637X/793/1/6
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4IW
UT WOS:000341301700006
ER

PT J
AU Robson, EI
   Ivison, RJ
   Smail, I
   Holland, WS
   Geach, JE
   Gibb, AG
   Riechers, D
   Ade, PAR
   Bintley, D
   Bock, J
   Chapin, EL
   Chapman, SC
   Clements, DL
   Conley, A
   Cooray, A
   Dunlop, JS
   Farrah, D
   Fich, M
   Fu, H
   Jenness, T
   Laporte, N
   Oliver, SJ
   Omont, A
   Perez-Fournon, I
   Scott, D
   Swinbank, AM
   Wardlow, J
AF Robson, E. I.
   Ivison, R. J.
   Smail, Ian
   Holland, W. S.
   Geach, J. E.
   Gibb, A. G.
   Riechers, D.
   Ade, P. A. R.
   Bintley, D.
   Bock, J.
   Chapin, E. L.
   Chapman, S. C.
   Clements, D. L.
   Conley, A.
   Cooray, A.
   Dunlop, J. S.
   Farrah, D.
   Fich, M.
   Fu, Hai
   Jenness, T.
   Laporte, N.
   Oliver, S. J.
   Omont, A.
   Perez-Fournon, I.
   Scott, Douglas
   Swinbank, A. M.
   Wardlow, J.
TI IMAGING THE ENVIRONMENT OF A z=6.3 SUBMILLIMETER GALAXY WITH SCUBA-2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: high-redshift; galaxies: starburst; infrared: galaxies; radio
   continuum: galaxies; submillimeter: galaxies
ID CLERK MAXWELL TELESCOPE; DEEP FIELD-SOUTH; STAR-FORMING GALAXIES; MU-M;
   EXTRAGALACTIC SURVEY; ELLIPTIC GALAXIES; STARBURST GALAXY; BOLOMETER
   CAMERA; NUMBER COUNTS; HERSCHEL
AB We describe a search for submillimeter emission in the vicinity of one of the most distant, luminous galaxies known, HerMES FLS3, at z = 6.34, exploiting it as a signpost to a potentially biased region of the early universe, as might be expected in hierarchical structure formation models. Imaging to the confusion limit with the innovative, wide-field submillimeter bolometer camera, SCUBA-2, we are sensitive to colder and/or less luminous galaxies in the surroundings of HFLS3. We use the Millennium Simulation to illustrate that HFLS3 may be expected to have companions if it is as massive as claimed, but find no significant evidence from the surface density of SCUBA-2 galaxies in its vicinity, or their colors, that HFLS3 marks an overdensity of dusty, star-forming galaxies. We cannot rule out the presence of dusty neighbors with confidence, but deeper 450 mu m imaging has the potential to more tightly constrain the redshifts of nearby galaxies, at least one of which likely lies at z greater than or similar to 5. If associations with HFLS3 can be ruled out, this could be taken as evidence that HFLS3 is less biased than a simple extrapolation of the Millennium Simulation may imply. This could suggest either that it represents a rare short-lived, but highly luminous, phase in the evolution of an otherwise typical galaxy, or that this system has suffered amplification due to a foreground gravitational lens and so is not as intrinsically luminous as claimed.
C1 [Robson, E. I.; Holland, W. S.] United Kingdom Astron Technol Ctr, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
   [Ivison, R. J.] European Space Observ, D-85748 Garching, Germany.
   [Ivison, R. J.; Holland, W. S.; Dunlop, J. S.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
   [Smail, Ian; Swinbank, A. M.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
   [Geach, J. E.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
   [Gibb, A. G.; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
   [Riechers, D.; Jenness, T.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
   [Ade, P. A. R.] Cardiff Univ, Astron & Instrumentat Grp, Cardiff CF10 3XQ, S Glam, Wales.
   [Bintley, D.] Joint Astron Ctr, Hilo, HI 96720 USA.
   [Bock, J.] CALTECH, Jet Prop Lab, Natl Aeronaut & Space Adm, Pasadena, CA 91109 USA.
   [Chapin, E. L.] European Space Astron Ctr, XMM Newton Sci Operat Ctr, E-28691 Madrid, Spain.
   [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, Boulder, CO 80309 USA.
   [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
   [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
   [Fich, M.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
   [Laporte, N.; Perez-Fournon, I.] Inst Astrofs Canarias, E-38200 Tenerife, Spain.
   [Oliver, S. J.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
   [Omont, A.] Univ Paris 06, IAP, UMR 7095, F-75014 Paris, France.
   [Omont, A.] CNRS, IAP, UMR 7095, F-75014 Paris, France.
   [Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
   [Wardlow, J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-1165 Copenhagen, Denmark.
RP Robson, EI (reprint author), United Kingdom Astron Technol Ctr, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
EM rob.ivison@gmail.com
RI Wardlow, Julie/C-9903-2015; Smail, Ian/M-5161-2013; Ivison,
   R./G-4450-2011; 
OI Wardlow, Julie/0000-0003-2376-8971; Smail, Ian/0000-0003-3037-257X;
   Ivison, R./0000-0001-5118-1313; Scott, Douglas/0000-0002-6878-9840;
   Jenness, Tim/0000-0001-5982-167X
FU European Research Council (ERC); COSMICISM; DUSTYGAL; UK's Science and
   Technology Facilities Council (STFC) [ST/I001573/1]; Leverhulme
   Fellowship; Royal Society/Wolfson Merit Award; Royal Society; Danish
   National Research Foundation; Canada Foundation for Innovation; CSA
   (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN
   (Spain); SNSB (Sweden); STFC, UKSA (UK); NASA (USA)
FX We thank John Helly for help with the Millennium Simulation. R.J.I. and
   I.R.S. acknowledge support from the European Research Council (ERC) in
   the form of Advanced Investigator programs, COSMICISM and DUSTYGAL,
   respectively. I.R.S. also acknowledges support from the UK's Science and
   Technology Facilities Council (STFC, ST/I001573/1), a Leverhulme
   Fellowship and a Royal Society/Wolfson Merit Award. J.E.G. acknowledges
   the Royal Society for support. The Dark Cosmology Centre is funded by
   the Danish National Research Foundation. The JCMT is operated by the
   Joint Astronomy Centre on behalf of STFC, the National Research Council
   of Canada and (until 2013 March 31) the Netherlands Organisation for
   Scientific Research. Additional funds for the construction of SCUBA-2
   were provided by the Canada Foundation for Innovation. Herschel is an
   ESA space observatory with science instruments provided by European-led
   Principal Investigator consortia and with important participation from
   NASA. SPIRE was developed by a consortium of institutes led by Cardiff
   University (UK) and including University of Lethbridge (Canada); NAOC
   (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain);
   Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL,
   UKATC, University of Sussex (UK); and Caltech, JPL, NHSC, University of
   Colorado (USA). This development has been supported by national funding
   agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI
   (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).
   The JCMT and Herschel data used in this paper can be obtained from the
   JCMT archive (http://www.jach.hawaii.edu/JCMT/archive) and the Herschel
   Database in Marseille, HeDaM, (http://hedam.oamp.fr/HerMES),
   respectively.
NR 39
TC 6
Z9 6
U1 0
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 20
PY 2014
VL 793
IS 1
AR 11
DI 10.1088/0004-637X/793/1/11
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4IW
UT WOS:000341301700011
ER

PT J
AU Walton, DJ
   Harrison, FA
   Grefenstette, BW
   Miller, JM
   Bachetti, M
   Barret, D
   Boggs, SE
   Christensen, FE
   Craig, WW
   Fabian, AC
   Fuerst, F
   Hailey, CJ
   Madsen, KK
   Parker, ML
   Ptak, A
   Rana, V
   Stern, D
   Webb, N
   Zhang, WW
AF Walton, D. J.
   Harrison, F. A.
   Grefenstette, B. W.
   Miller, J. M.
   Bachetti, M.
   Barret, D.
   Boggs, S. E.
   Christensen, F. E.
   Craig, W. W.
   Fabian, A. C.
   Fuerst, F.
   Hailey, C. J.
   Madsen, K. K.
   Parker, M. L.
   Ptak, A.
   Rana, V.
   Stern, D.
   Webb, N.
   Zhang, W. W.
TI BROADBAND X-RAY SPECTRA OF THE ULTRALUMINOUS X-RAY SOURCE HOLMBERG IX
   X-1 OBSERVED WITH NuSTAR, XMM-NEWTON, AND SUZAKU
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; X-rays: binaries; X-rays: individual (Holmberg IX
   X-1)
ID SUPER-EDDINGTON ACCRETION; PHOTON IMAGING CAMERA; MASS BLACK-HOLES; NGC
   5408 X-1; CYGNUS X-1; SOFT STATE; DISKS; VARIABILITY; REFLECTION;
   EMISSION
AB We present results from the coordinated broadband X-ray observations of the extreme ultraluminous X-ray source Holmberg IX X-1 performed by NuSTAR, XMM-Newton, and Suzaku in late 2012. These observations provide the first high-quality spectra of Holmberg IX X-1 above 10 keV to date, extending the X-ray coverage of this remarkable source up to similar to 30 keV. Broadband observations were undertaken at two epochs, between which Holmberg IX X-1 exhibited both flux and strong spectral variability, increasing in luminosity from L-X = (1.90 +/- 0.03) x 10(40) erg s(-1) to L-X = (3.35 +/- 0.03) x 10(40) erg s(-1). Neither epoch exhibits a spectrum consistent with emission from the standard low/hard accretion state seen in Galactic black hole binaries, which would have been expected if Holmberg IX X-1 harbors a truly massive black hole accreting at substantially sub-Eddington accretion rates. The NuSTAR data confirm that the curvature observed previously in the 3-10 keV bandpass does represent a true spectral cutoff. During each epoch, the spectrum appears to be dominated by two optically thick thermal components, likely associated with an accretion disk. The spectrum also shows some evidence for a nonthermal tail at the highest energies, which may further support this scenario. The available data allow for either of the two thermal components to dominate the spectral evolution, although both scenarios require highly nonstandard behavior for thermal accretion disk emission.
C1 [Walton, D. J.; Harrison, F. A.; Grefenstette, B. W.; Fuerst, F.; Madsen, K. K.; Rana, V.; Stern, D.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
   [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
   [Bachetti, M.; Barret, D.; Webb, N.] Univ Toulouse, UPS, OMP, IRAP, Toulouse, France.
   [Bachetti, M.; Barret, D.; Webb, N.] CNRS, IRAP, F-31028 Toulouse 4, France.
   [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2088 Lyngby, Denmark.
   [Fabian, A. C.; Parker, M. L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
   [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Ptak, A.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Walton, DJ (reprint author), CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
EM dwalton@srl.caltech.edu
RI Boggs, Steven/E-4170-2015; XRAY, SUZAKU/A-1808-2009; 
OI Boggs, Steven/0000-0001-9567-4224; Bachetti, Matteo/0000-0002-4576-9337;
   Rana, Vikram/0000-0003-1703-8796
FU NASA [NNG08FD60C]; XMM-Newton; ESA; Suzaku; space agencies of Japan
   (JAXA); USA (NASA); Centre National d'Etudes Spatiales (CNES); ESA
   Member States
FX The authors would like to thank the referee for providing useful
   feedback, which helped to improve the manuscript. This research has made
   use of data obtained with the NuSTAR mission, a project led by the
   California Institute of Technology (Caltech), managed by the Jet
   Propulsion Laboratory (JPL) and funded by NASA, XMM-Newton, an ESA
   science mission with instruments and contributions directly funded by
   ESA Member States and NASA, and Suzaku, a collaborative mission between
   the space agencies of Japan (JAXA) and the USA (NASA). We thank the
   NuSTAR Operations, Software, and Calibration teams for support with the
   execution and analysis of these observations. This research was
   supported under NASA grant No. NNG08FD60C, and has made use of the
   NuSTAR Data Analysis Software (NUSTARDAS), jointly developed by the ASI
   Science Data Center (ASDC, Italy) and Caltech (USA). We also made use of
   the NASA/IPAC Extragalactic Database (NED), which is operated by JPL,
   Caltech, under contract with NASA. Many of the figures included in this
   work have been produced with the Veusz plotting package:
   http://home.gna.org/veusz, written and maintained by Jeremy Sanders. DB
   and MB are grateful to the Centre National d'Etudes Spatiales (CNES) for
   funding their activities.
NR 76
TC 41
Z9 41
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2014
VL 793
IS 1
AR 21
DI 10.1088/0004-637X/793/1/21
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4IW
UT WOS:000341301700021
ER

PT J
AU Wu, J
   Bussmann, RS
   Tsai, CW
   Petric, A
   Blain, A
   Eisenhardt, PRM
   Bridge, CR
   Benford, DJ
   Stern, D
   Assef, RJ
   Gelino, CR
   Moustakas, L
   Wright, EL
AF Wu, Jingwen
   Bussmann, R. Shane
   Tsai, Chao-Wei
   Petric, Andreea
   Blain, Andrew
   Eisenhardt, Peter R. M.
   Bridge, Carrie R.
   Benford, Dominic J.
   Stern, Daniel
   Assef, Roberto J.
   Gelino, Christopher R.
   Moustakas, Leonidas
   Wright, Edward L.
TI INTERFEROMETRIC FOLLOW-UP OF WISE HYPER-LUMINOUS HOT, DUST-OBSCURED
   GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: formation; galaxies: high-redshift; galaxies: individual (WISE
   J014946.17+235014.5,WISE J181417.29+341224.9,WISE J223810.20+265319.7);
   galaxies: ISM; galaxies: starburst; infrared: galaxies
ID SIMILAR-TO 2; SPACE-TELESCOPE MORPHOLOGIES; ADAPTIVE OPTICS SYSTEM;
   HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; QUASAR HOST GALAXIES;
   SUBMILLIMETER GALAXIES; MOLECULAR GAS; CO EMISSION; INFRARED
   LUMINOSITIES
AB The Wide-field Infrared Survey Explorer (WISE) has discovered an extraordinary population of hyper-luminous dusty galaxies that are faint in the two bluer passbands (3.4 mu m and 4.6 mu m) but are bright in the two redder passbands of WISE (12 mu m and 22 mu m). We report on initial follow-up observations of three of these hot, dust-obscured galaxies, or Hot DOGs, using the Combined Array for Research in Millimeter-wave Astronomy and the Submillimeter Array interferometer arrays at submillimeter/millimeter wavelengths. We report continuum detections at similar to 1.3 mm of two sources (WISE J014946.17+235014.5 and WISE J223810.20+265319.7, hereafter W0149+2350 and W2238+2653, respectively), and upper limits to CO line emission at 3 mm in the observed frame for two sources (W0149+2350 and WISE J181417.29+341224.8, hereafter W1814+3412). The 1.3 mm continuum images have a resolution of 1 ''-2 '' and are consistent with single point sources. We estimate the masses of cold dust are 2.0 x 10(8) M-circle dot for W0149+2350 and 3.9 x 10(8) M-circle dot for W2238+2653, comparable to cold dust masses of luminous quasars. We obtain 2 sigma upper limits to the molecular gas masses traced by CO, which are 3.3 x 1010 M-circle dot and 2.3 x 10(10) M-circle dot for W0149+2350 and W1814+3412, respectively. We also present high-resolution, near-IR imaging with the WFC3 on the Hubble Space Telescope for W0149+2653 and with NIRC2 on Keck for W2238+2653. The near-IR images show morphological structure dominated by a single, centrally condensed source with effective radius less than 4 kpc. No signs of gravitational lensing are evident.
C1 [Wu, Jingwen; Wright, Edward L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
   [Bussmann, R. Shane] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Bussmann, R. Shane] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
   [Tsai, Chao-Wei; Moustakas, Leonidas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Petric, Andreea] Astron Inst, Honolulu, HI 96822 USA.
   [Blain, Andrew] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
   [Bridge, Carrie R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
   [Benford, Dominic J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Assef, Roberto J.] Univ Diego Portales, Fac Ingn, Santiago, Chile.
   [Gelino, Christopher R.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
RP Wu, J (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
EM jingwen@astro.ucla.edu
RI Benford, Dominic/D-4760-2012; 
OI Benford, Dominic/0000-0002-9884-4206; Moustakas,
   Leonidas/0000-0003-3030-2360
FU National Aeronautics and Space Administration; National Science
   Foundation; CARMA partner universities; NASA [NAS 5-26555]; W.M. Keck
   Foundation [AST 90-15755]; Gemini-CONICYT [32120009]
FX This publication makes use of data products from the Widef-ield Infrared
   Survey Explorer, which is a joint project of the University of
   California, Los Angeles, and the Jet Propulsion Laboratory/California
   Institute of Technology, funded by the National Aeronautics and Space
   Administration. This work is based on observations made with the
   Combined Array for Research in Millimeter-wave Astronomy (CARMA).
   Support for CARMA construction was derived from the states of
   California, Illinois, and Maryland, the James S. McDonnell Foundation,
   the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L.
   Norris Foundation, the University of Chicago, the Associates of the
   California Institute of Technology, and the National Science Foundation.
   Ongoing CARMA development and operations are supported by the National
   Science Foundation under a cooperative agreement, and by the CARMA
   partner universities. This work is also based on observations made with
   the Submillimeter Array (SMA). 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. Some of the data are 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. Some of the data presented herein were obtained at
   the W.M. Keck Observatory, which is operated as a scientific partnership
   among Caltech, the University of California and NASA. The Keck
   Observatory was made possible by the generous financial support of the
   W.M. Keck Foundation. This work uses data from Herschel. Herschel is an
   ESA space observatory with science instruments provided by European-led
   Principal Investigator consortia and with important participation from
   NASA. This work uses data from CSO, which is operated by the California
   Institute of Technology under funding from the National Science
   Foundation, contract AST 90-15755. R.J.A. was supported by
   Gemini-CONICYT grant number 32120009.
NR 81
TC 12
Z9 12
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2014
VL 793
IS 1
AR 8
DI 10.1088/0004-637X/793/1/8
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4IW
UT WOS:000341301700008
ER

PT J
AU Kurczynski, P
   Gawiser, E
   Rafelski, M
   Teplitz, HI
   Acquaviva, V
   Brown, TM
   Coe, D
   de Mello, DF
   Finkelstein, SL
   Grogin, NA
   Koekemoer, AM
   Lee, KS
   Scarlata, C
   Siana, BD
AF Kurczynski, Peter
   Gawiser, Eric
   Rafelski, Marc
   Teplitz, Harry I.
   Acquaviva, Viviana
   Brown, Thomas M.
   Coe, Dan
   de Mello, Duilia F.
   Finkelstein, Steven L.
   Grogin, Norman A.
   Koekemoer, Anton M.
   Lee, Kyoung-Soo
   Scarlata, Claudia
   Siana, Brian D.
TI THE UV CONTINUUM OF z > 1 STAR-FORMING GALAXIES IN THE HUBBLE
   ULTRAVIOLET ULTRADEEP FIELD
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmology: observations; galaxies: evolution; galaxies: formation;
   galaxies: high; redshift galaxies: structure
ID LYMAN BREAK GALAXIES; HIGH-REDSHIFT GALAXIES; FORMATION RATE DENSITY;
   SIMILAR-TO 2; RELEASE SCIENCE OBSERVATIONS; DEEP FIELD; STELLAR
   POPULATIONS; STARBURST GALAXIES; DUST ATTENUATION; LUMINOSITY FUNCTION
AB We estimate the UV continuum slope, beta, for 923 galaxies in the range 1 < z < 8 in the Hubble Ultradeep Field (HUDF). These data include 460 galaxies at 1 < z < 2 down to an absolute magnitude M-UV = -14(similar to 0.006L(z=1)(*); 0.02L(z=0)(*)), comparable to dwarf galaxies in the local universe. We combine deep HST/UVIS photometry in F225W, F275W, F336W wavebands (UVUDF) with recent data from HST/WFC3/IR (HUDF12). Galaxies in the range 1 < z < 2 are significantly bluer than local dwarf galaxies. We find theirmean (median) values (beta)= -1.382(-1.830)+/- 0.002 (random)+/- 0.1 (systematic). We find comparable scatter in beta (standard deviation = 0.43) to local dwarf galaxies and 30% larger scatter than z > 2 galaxies. We study the trends of beta with redshift and absolute magnitude for binned sub-samples and find a modest color-magnitude relation, d beta/dM= -0.11 +/- 0.01, and no evolution in d beta/dM with redshift. A modest increase in dust reddening with redshift and luminosity, Delta E(B -V) similar to 0.1, and a comparable increase in the dispersion of dust reddening atz < 2, appears likely to explain the observed trends. At z > 2, we find trends that are consistent with previous works; combining our data with the literature in the range 1 < z < 8, we find a color evolution with redshift, d beta/dz=-0.09 +/- 0.01 for low luminosity (0.05 L*z=3), and d beta/dz = -0.06 +/- 0.01 for medium luminosity (0.25 L-z=3(*)) galaxies.
C1 [Kurczynski, Peter; Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
   [Rafelski, Marc] NASA, Goddard Space Flight Ctr, Postdoctoral Program Fellow, Greenbelt, MD 20771 USA.
   [Teplitz, Harry I.] Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
   [Acquaviva, Viviana] New York City Coll Technol, Brooklyn, NY 11201 USA.
   [Brown, Thomas M.; Coe, Dan; Grogin, Norman A.; Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [de Mello, Duilia F.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Lab Observat Cosmol, Greenbelt, MD 20771 USA.
   [de Mello, Duilia F.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
   [Finkelstein, Steven L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
   [Lee, Kyoung-Soo] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
   [Scarlata, Claudia] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
   [Siana, Brian D.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
RP Kurczynski, P (reprint author), Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
OI Gawiser, Eric/0000-0003-1530-8713; Koekemoer, Anton/0000-0002-6610-2048;
   Brown, Thomas/0000-0002-1793-9968
FU HST Program [GO-12534]; NASA through grants from the Space Telescope
   Science Institute; National Science Foundation [1055919]
FX The authors wish to thank the anonymous referee for comments that
   greatly improved this manuscript. Support for HST Program GO-12534 was
   provided by NASA through grants from the Space Telescope Science
   Institute, which is operated by the Association of Universities for
   Research in Astronomy, Inc., under NASA contract NAS5-2655. This
   material is based upon work supported by the National Science Foundation
   under grant no. 1055919.
NR 43
TC 6
Z9 6
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 2014
VL 793
IS 1
AR L5
DI 10.1088/2041-8205/793/1/L5
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4MP
UT WOS:000341313700005
ER

PT J
AU Romani, RW
   Filippenko, AV
   Cenko, SB
AF Romani, Roger W.
   Filippenko, Alexei V.
   Cenko, S. Bradley
TI 2FGL J1653.6-0159: A NEW LOW IN EVAPORATING PULSAR BINARY PERIODS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE gamma rays: stars; pulsars: general
ID GAMMA-RAY PULSARS; MILLISECOND PULSAR; FERMI-LAT; TELESCOPE; DISCOVERY;
   COMPANION; SEARCHES; CATALOG
AB We have identified an optical binary with orbital period P-b = 4488 s as the probable counterpart of the Fermi source 2FGL J1653.6-0159. Although pulsations have not yet been detected, the source properties are consistent with an evaporating millisecond pulsar binary; this P-b = 75 minutes is the record low for a spin-powered system. The heated side of the companion shows coherent radial-velocity variations, with amplitude K = 666.9 +/- 7.5 km s(-1) for a large mass function of f (M) = 1.60 +/- 0.05 M-circle dot. This heating suggests a pulsar luminosity similar to 3 x 10(34) erg s(-1). The colors and spectra show an additional blue component dominating at binary minimum. Its origin is, at present, unclear. This system is similar to PSR J1311-3430, with a low-mass H-depleted companion, a dense shrouding wind and, likely, a large pulsar mass.
C1 [Romani, Roger W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
   [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 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.
RP Romani, RW (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
EM rwr@astro.stanford.edu
FU NASA [NNX11AO44G]; Richard & Rhoda Goldman Fund; Christopher R. Redlich
   Fund; TABASGO Foundation; NSF [AST-1211916]; W. M. Keck Foundation
FX . We thank Sasha Brownsberger and Matt Stadnik for assistance with the
   photometric observations, and Melissa Graham, Patrick L. Kelly, and
   WeiKang Zheng for assistance with the spectroscopic observations. This
   work was supported in part by NASA grant NNX11AO44G. A. V. F. was
   supported by the Richard & Rhoda Goldman Fund, the Christopher R.
   Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. This
   research is based in part on observations obtained at the Southern
   Astrophysical Research (SOAR) telescope, which is a joint project of the
   Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da Republica
   Federativa do Brasil, the U. S. National Optical Astronomy Observatory
   (NOAO), the University of North Carolina at Chapel Hill (UNC), and
   Michigan State University (MSU). 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.
NR 21
TC 6
Z9 6
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2014
VL 793
IS 1
AR L20
DI 10.1088/2041-8205/793/1/L20
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO4MP
UT WOS:000341313700020
ER

PT J
AU Etienne, ZB
   Baker, JG
   Paschalidis, V
   Kelly, BJ
   Shapiro, SL
AF Etienne, Zachariah B.
   Baker, John G.
   Paschalidis, Vasileios
   Kelly, Bernard J.
   Shapiro, Stuart L.
TI Improved moving puncture gauge conditions for compact binary evolutions
SO PHYSICAL REVIEW D
LA English
DT Article
ID BLACK-HOLES; NUMERICAL RELATIVITY; GRAVITATIONAL-WAVES; INITIAL DATA
AB Robust gauge conditions are critically important to the stability and accuracy of numerical relativity (NR) simulations involving compact objects. Most of the NR community use the highly robust-though decade-old-moving-puncture (MP) gauge conditions for such simulations. It has been argued that in binary black hole evolutions adopting this gauge, noise generated near adaptive-mesh-refinement (AMR) boundaries does not converge away cleanly with increasing resolution, severely limiting gravitational waveform accuracy at computationally feasible resolutions. We link this noise to a sharp (short-wavelength), initial outgoing gauge wave crossing into progressively lower resolution AMR grids and present improvements to the standard MP gauge conditions that focus on stretching, smoothing, and more rapidly settling this outgoing wave. Our best gauge choice greatly reduces gravitational waveform noise during inspiral, yielding less fluctuation in convergence order and similar to 40% lower waveform phase and amplitude errors at typical resolutions. Noise in other physical quantities of interest is also reduced, and constraint violations drop by more than an order of magnitude. We expect these improvements will carry over to simulations of all types of compact binary systems, as well as other N + 1 formulations of gravity for which MP-like gauge conditions can be chosen.
C1 [Etienne, Zachariah B.; Baker, John G.; Kelly, Bernard J.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
   [Etienne, Zachariah B.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
   [Etienne, Zachariah B.; Baker, John G.; Kelly, Bernard J.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
   [Etienne, Zachariah B.] W Virginia Univ, Dept Math, Morgantown, WV 26506 USA.
   [Paschalidis, Vasileios; Shapiro, Stuart L.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
   [Kelly, Bernard J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
   [Shapiro, Stuart L.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
   [Shapiro, Stuart L.] Univ Illinois, NCSA, Urbana, IL 61801 USA.
   [Kelly, Bernard J.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
RP Etienne, ZB (reprint author), Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
EM zetienne@umd.edu
OI Kelly, Bernard/0000-0002-3326-4454
FU NSF [PHY-0963136, PHY-1300903, OCI-1053575]; NASA at the University of
   Illinois at Urbana-Champaign [NNX11AE11G, NNX13AH44G]; NASA
   [09-ATP09-0136, 11-ATP-046]; Fortner Fellowship at UIUC; National
   Science Foundation [OCI 07-25070]; state of Illinois
FX This paper was supported in part by NSF Grants PHY-0963136 and
   PHY-1300903 as well as NASA Grants NNX11AE11G and NNX13AH44G at the
   University of Illinois at Urbana-Champaign. B. J. K. and J. G. B. were
   supported by NASA grants 09-ATP09-0136 and 11-ATP-046. V. P. gratefully
   acknowledges support from a Fortner Fellowship at UIUC. This work used
   the Extreme Science and Engineering Discovery Environment (XSEDE), which
   is supported by NSF grant number OCI-1053575. A significant portion of
   the calculations presented here were performed as part of the Blue
   Waters sustained-petascale computing project, which is supported by the
   National Science Foundation (award number OCI 07-25070) and the state of
   Illinois. Blue Waters is a joint effort of the University of Illinois at
   Urbana-Champaign and its National Center for Supercomputing
   Applications.
NR 57
TC 3
Z9 3
U1 0
U2 0
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 SEP 19
PY 2014
VL 90
IS 6
AR 064032
DI 10.1103/PhysRevD.90.064032
PG 25
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AP5TZ
UT WOS:000342142900001
ER

PT J
AU Bormann, KJ
   Evans, JP
   McCabe, MF
AF Bormann, Kathryn J.
   Evans, Jason P.
   McCabe, Matthew F.
TI Constraining snowmelt in a temperature-index model using simulated snow
   densities
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Snow density; Snow modelling; Melt factor; Degree-day factor; Warm
   maritime snowpack dynamics; Snow depth
ID CLIMATE-CHANGE; WINTER PRECIPITATION; WATER EQUIVALENT; MELT
   SIMULATIONS; SOLAR-RADIATION; RUNOFF MODEL; SKI RESORTS; AUSTRALIA;
   ALPS; VARIABILITY
AB Current snowmelt parameterisation schemes are largely untested in warmer maritime snowfields, where physical snow properties can differ substantially from the more common colder snow environments. Physical properties such as snow density influence the thermal properties of snow layers and are likely to be important for snowmelt rates. Existing methods for incorporating physical snow properties into temperature-index models (TIMs) require frequent snow density observations. These observations are often unavailable in less monitored snow environments. In this study, previous techniques for end-of-season snow density estimation (Bormann et al., 2013) were enhanced and used as a basis for generating daily snow density data from climate inputs. When evaluated against 2970 observations, the snow density model outperforms a regionalised density-time curve reducing biases from -0.027 g cm(-3) to -0.004 g cm(-3) (7%). The simulated daily densities were used at 13 sites in the warmer maritime snowfields of Australia to parameterise snowmelt estimation. With absolute snow water equivalent (SWE) errors between 100 and 136 mm, the snow model performance was generally lower in the study region than that reported for colder snow environments, which may be attributed to high annual variability. Model performance was strongly dependent on both calibration and the adjustment for precipitation undercatch errors, which influenced model calibration parameters by 150-200%. Comparison of the density-based snowmelt algorithm against a typical temperature-index model revealed only minor differences between the two snowmelt schemes for estimation of SWE. However, when the model was evaluated against snow depths, the new scheme reduced errors by up to 50%, largely due to improved SWE to depth conversions. While this study demonstrates the use of simulated snow density in snowmelt parameterisation, the snow density model may also be of broad interest for snow depth to SWE conversion. Overall, the study responds to recent calls for broader testing of TIMs across different snow environments, improves existing snow modelling in Australia and proposes a new method for introducing physically-based constraints on snowmelt rates in data-poor regions. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Bormann, Kathryn J.; Evans, Jason P.] Univ New S Wales, Climate Change Res Ctr, Sydney, NSW, Australia.
   [Bormann, Kathryn J.; Evans, Jason P.] Univ New S Wales, ARC Ctr Excellence Climate Syst Sci, Sydney, NSW, Australia.
   [Bormann, Kathryn J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [McCabe, Matthew F.] King Abdullah Univ Sci & Technol, Water Desalinat & Reuse Ctr, Thuwal, Saudi Arabia.
RP Bormann, KJ (reprint author), Jet Prop Lab, 4800 Oak Grove Dr,MS 233-304, Pasadena, CA 91101 USA.
EM katbormann@gmail.com
RI Evans, Jason/F-3716-2011; McCabe, Matthew/G-5194-2011
OI Evans, Jason/0000-0003-1776-3429; McCabe, Matthew/0000-0002-1279-5272
FU Australian Research Council [FT110100576]
FX We thank Andrew Nolan, Jason Venables, Shane Bilish and Johanna Speirs
   at Snowy Hydro Limited for their cooperation in providing the data along
   with comments on the manuscript, and Tristan Sasse for valuable
   suggestions during manuscript preparation and planning. J.P. Evans was
   supported by an Australian Research Council Future Fellowship
   (FT110100576).
NR 58
TC 4
Z9 4
U1 1
U2 23
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 19
PY 2014
VL 517
BP 652
EP 667
DI 10.1016/j.jhydrol.2014.05.073
PG 16
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA AO0CP
UT WOS:000340977000056
ER

PT J
AU Accardo, L
   Aguilar, M
   Aisa, D
   Alpat, B
   Alvino, A
   Ambrosi, G
   Andeen, K
   Arruda, L
   Attig, N
   Azzarello, P
   Bachlechner, A
   Barao, F
   Barrau, A
   Barrin, L
   Bartoloni, A
   Basara, L
   Battarbee, M
   Battiston, R
   Bazo, J
   Becker, U
   Behlmann, M
   Beischer, B
   Berdugo, J
   Bertucci, B
   Bigongiari, G
   Bindi, V
   Bizzaglia, S
   Bizzarri, M
   Boella, G
   de Boer, W
   Bollweg, K
   Bonnivard, V
   Borgia, B
   Borsini, S
   Boschini, MJ
   Bourquin, M
   Burger, J
   Cadoux, F
   Cai, XD
   Capell, M
   Caroff, S
   Carosi, G
   Casaus, J
   Cascioli, V
   Castellini, G
   Cernuda, I
   Cerreta, D
   Cervelli, F
   Chae, MJ
   Chang, YH
   Chen, AI
   Chen, H
   Cheng, GM
   Chen, HS
   Cheng, L
   Chikanian, A
   Chou, HY
   Choumilov, E
   Choutko, V
   Chung, CH
   Cindolo, F
   Clark, C
   Clavero, R
   Coignet, G
   Consolandi, C
   Contin, A
   Corti, C
   Coste, B
   Cui, Z
   Dai, M
   Delgado, C
   Della Torre, S
   Demirkoz, MB
   Derome, L
   Di Falco, S
   Di Masso, L
   Dimiccoli, F
   Diaz, C
   von Doetinchem, P
   Du, WJ
   Duranti, M
   D'Urso, D
   Eline, A
   Eppling, FJ
   Eronen, T
   Fan, YY
   Farnesini, L
   Feng, J
   Fiandrini, E
   Fiasson, A
   Finch, E
   Fisher, P
   Galaktionov, Y
   Gallucci, G
   Garcia, B
   Garcia-Lopez, R
   Gast, H
   Gebauer, I
   Gervasi, M
   Ghelfi, A
   Gillard, W
   Giovacchini, F
   Goglov, P
   Gong, J
   Goy, C
   Grabski, V
   Grandi, D
   Graziani, M
   Guandalini, C
   Guerri, I
   Guo, KH
   Haas, D
   Habiby, M
   Haino, S
   Han, KC
   He, ZH
   Heil, M
   Henning, R
   Hoffman, J
   Hsieh, TH
   Huang, ZC
   Huh, C
   Incagli, M
   Ionica, M
   Jang, WY
   Jinchi, H
   Kanishev, K
   Kim, GN
   Kim, KS
   Kirn, T
   Kossakowski, R
   Kounina, O
   Kounine, A
   Koutsenko, V
   Krafczyk, MS
   Kunz, S
   La Vacca, G
   Laudi, E
   Laurenti, G
   Lazzizzera, I
   Lebedev, A
   Lee, HT
   Lee, SC
   Leluc, C
   Levi, G
   Li, HL
   Li, JQ
   Li, Q
   Li, Q
   Li, TX
   Li, W
   Li, Y
   Li, ZH
   Li, ZY
   Lim, S
   Lin, CH
   Lipari, P
   Lippert, T
   Liu, D
   Liu, H
   Lolli, M
   Lomtadze, T
   Lu, MJ
   Lu, YS
   Luebelsmeyer, K
   Luo, F
   Luo, JZ
   Lv, SS
   Majka, R
   Malinin, A
   Mana, C
   Marin, J
   Martin, T
   Martinez, G
   Masi, N
   Massera, F
   Maurin, D
   Menchaca-Rocha, A
   Meng, Q
   Mo, DC
   Monreal, B
   Morescalchi, L
   Mott, P
   Muller, M
   Ni, JQ
   Nikonov, N
   Nozzoli, F
   Nunes, P
   Obermeier, A
   Oliva, A
   Orcinha, M
   Palmonari, F
   Palomares, C
   Paniccia, M
   Papi, A
   Pauluzzi, M
   Pedreschi, E
   Pensotti, S
   Pereira, R
   Pilastrini, R
   Pilo, F
   Piluso, A
   Pizzolotto, C
   Plyaskin, V
   Pohl, M
   Poireau, V
   Postaci, E
   Putze, A
   Quadrani, L
   Qi, XM
   Rancoita, PG
   Rapin, D
   Ricol, JS
   Rodriguez, I
   Rosier-Lees, S
   Rossi, L
   Rozhkov, A
   Rozza, D
   Rybka, G
   Sagdeev, R
   Sandweiss, J
   Saouter, P
   Sbarra, C
   Schael, S
   Schmidt, SM
   Schuckardt, D
   von Dratzig, AS
   Schwering, G
   Scolieri, G
   Seo, ES
   Shan, BS
   Shan, YH
   Shi, JY
   Shi, XY
   Shi, YM
   Siedenburg, T
   Son, D
   Spada, F
   Spinella, F
   Sun, W
   Sun, WH
   Tacconi, M
   Tang, CP
   Tang, XW
   Tang, ZC
   Tao, L
   Tescaro, D
   Ting, SCC
   Ting, SM
   Tomassetti, N
   Torsti, J
   Turkoglu, C
   Urban, T
   Vagelli, V
   Valente, E
   Vannini, C
   Valtonen, E
   Vaurynovich, S
   Vecchi, M
   Velasco, M
   Vialle, JP
   Vitale, V
   Volpini, G
   Wang, LQ
   Wang, QL
   Wang, RS
   Wang, X
   Wang, ZX
   Weng, ZL
   Whitman, K
   Wienkenhover, J
   Wu, H
   Wu, KY
   Xia, X
   Xie, M
   Xie, S
   Xiong, RQ
   Xin, GM
   Xu, NS
   Xu, W
   Yan, Q
   Yang, J
   Yang, M
   Ye, QH
   Yi, H
   Yu, YJ
   Yu, ZQ
   Zeissler, S
   Zhang, JH
   Zhang, MT
   Zhang, XB
   Zhang, Z
   Zheng, ZM
   Zhou, F
   Zhuang, HL
   Zhukov, V
   Zichichi, A
   Zimmermann, N
   Zuccon, P
   Zurbach, C
AF Accardo, L.
   Aguilar, M.
   Aisa, D.
   Alpat, B.
   Alvino, A.
   Ambrosi, G.
   Andeen, K.
   Arruda, L.
   Attig, N.
   Azzarello, P.
   Bachlechner, A.
   Barao, F.
   Barrau, A.
   Barrin, L.
   Bartoloni, A.
   Basara, L.
   Battarbee, M.
   Battiston, R.
   Bazo, J.
   Becker, U.
   Behlmann, M.
   Beischer, B.
   Berdugo, J.
   Bertucci, B.
   Bigongiari, G.
   Bindi, V.
   Bizzaglia, S.
   Bizzarri, M.
   Boella, G.
   de Boer, W.
   Bollweg, K.
   Bonnivard, V.
   Borgia, B.
   Borsini, S.
   Boschini, M. J.
   Bourquin, M.
   Burger, J.
   Cadoux, F.
   Cai, X. D.
   Capell, M.
   Caroff, S.
   Carosi, G.
   Casaus, J.
   Cascioli, V.
   Castellini, G.
   Cernuda, I.
   Cerreta, D.
   Cervelli, F.
   Chae, M. J.
   Chang, Y. H.
   Chen, A. I.
   Chen, H.
   Cheng, G. M.
   Chen, H. S.
   Cheng, L.
   Chikanian, A.
   Chou, H. Y.
   Choumilov, E.
   Choutko, V.
   Chung, C. H.
   Cindolo, F.
   Clark, C.
   Clavero, R.
   Coignet, G.
   Consolandi, C.
   Contin, A.
   Corti, C.
   Coste, B.
   Cui, Z.
   Dai, M.
   Delgado, C.
   Della Torre, S.
   Demirkoez, M. B.
   Derome, L.
   Di Falco, S.
   Di Masso, L.
   Dimiccoli, F.
   Diaz, C.
   von Doetinchem, P.
   Du, W. J.
   Duranti, M.
   D'Urso, D.
   Eline, A.
   Eppling, F. J.
   Eronen, T.
   Fan, Y. Y.
   Farnesini, L.
   Feng, J.
   Fiandrini, E.
   Fiasson, A.
   Finch, E.
   Fisher, P.
   Galaktionov, Y.
   Gallucci, G.
   Garcia, B.
   Garcia-Lopez, R.
   Gast, H.
   Gebauer, I.
   Gervasi, M.
   Ghelfi, A.
   Gillard, W.
   Giovacchini, F.
   Goglov, P.
   Gong, J.
   Goy, C.
   Grabski, V.
   Grandi, D.
   Graziani, M.
   Guandalini, C.
   Guerri, I.
   Guo, K. H.
   Haas, D.
   Habiby, M.
   Haino, S.
   Han, K. C.
   He, Z. H.
   Heil, M.
   Henning, R.
   Hoffman, J.
   Hsieh, T. H.
   Huang, Z. C.
   Huh, C.
   Incagli, M.
   Ionica, M.
   Jang, W. Y.
   Jinchi, H.
   Kanishev, K.
   Kim, G. N.
   Kim, K. S.
   Kirn, Th.
   Kossakowski, R.
   Kounina, O.
   Kounine, A.
   Koutsenko, V.
   Krafczyk, M. S.
   Kunz, S.
   La Vacca, G.
   Laudi, E.
   Laurenti, G.
   Lazzizzera, I.
   Lebedev, A.
   Lee, H. T.
   Lee, S. C.
   Leluc, C.
   Levi, G.
   Li, H. L.
   Li, J. Q.
   Li, Q.
   Li, Q.
   Li, T. X.
   Li, W.
   Li, Y.
   Li, Z. H.
   Li, Z. Y.
   Lim, S.
   Lin, C. H.
   Lipari, P.
   Lippert, T.
   Liu, D.
   Liu, H.
   Lolli, M.
   Lomtadze, T.
   Lu, M. J.
   Lu, Y. S.
   Luebelsmeyer, K.
   Luo, F.
   Luo, J. Z.
   Lv, S. S.
   Majka, R.
   Malinin, A.
   Mana, C.
   Marin, J.
   Martin, T.
   Martinez, G.
   Masi, N.
   Massera, F.
   Maurin, D.
   Menchaca-Rocha, A.
   Meng, Q.
   Mo, D. C.
   Monreal, B.
   Morescalchi, L.
   Mott, P.
   Mueller, M.
   Ni, J. Q.
   Nikonov, N.
   Nozzoli, F.
   Nunes, P.
   Obermeier, A.
   Oliva, A.
   Orcinha, M.
   Palmonari, F.
   Palomares, C.
   Paniccia, M.
   Papi, A.
   Pauluzzi, M.
   Pedreschi, E.
   Pensotti, S.
   Pereira, R.
   Pilastrini, R.
   Pilo, F.
   Piluso, A.
   Pizzolotto, C.
   Plyaskin, V.
   Pohl, M.
   Poireau, V.
   Postaci, E.
   Putze, A.
   Quadrani, L.
   Qi, X. M.
   Rancoita, P. G.
   Rapin, D.
   Ricol, J. S.
   Rodriguez, I.
   Rosier-Lees, S.
   Rossi, L.
   Rozhkov, A.
   Rozza, D.
   Rybka, G.
   Sagdeev, R.
   Sandweiss, J.
   Saouter, P.
   Sbarra, C.
   Schael, S.
   Schmidt, S. M.
   Schuckardt, D.
   von Dratzig, A. Schulz
   Schwering, G.
   Scolieri, G.
   Seo, E. S.
   Shan, B. S.
   Shan, Y. H.
   Shi, J. Y.
   Shi, X. Y.
   Shi, Y. M.
   Siedenburg, T.
   Son, D.
   Spada, F.
   Spinella, F.
   Sun, W.
   Sun, W. H.
   Tacconi, M.
   Tang, C. P.
   Tang, X. W.
   Tang, Z. C.
   Tao, L.
   Tescaro, D.
   Ting, Samuel C. C.
   Ting, S. M.
   Tomassetti, N.
   Torsti, J.
   Tuerkoglu, C.
   Urban, T.
   Vagelli, V.
   Valente, E.
   Vannini, C.
   Valtonen, E.
   Vaurynovich, S.
   Vecchi, M.
   Velasco, M.
   Vialle, J. P.
   Vitale, V.
   Volpini, G.
   Wang, L. Q.
   Wang, Q. L.
   Wang, R. S.
   Wang, X.
   Wang, Z. X.
   Weng, Z. L.
   Whitman, K.
   Wienkenhoever, J.
   Wu, H.
   Wu, K. Y.
   Xia, X.
   Xie, M.
   Xie, S.
   Xiong, R. Q.
   Xin, G. M.
   Xu, N. S.
   Xu, W.
   Yan, Q.
   Yang, J.
   Yang, M.
   Ye, Q. H.
   Yi, H.
   Yu, Y. J.
   Yu, Z. Q.
   Zeissler, S.
   Zhang, J. H.
   Zhang, M. T.
   Zhang, X. B.
   Zhang, Z.
   Zheng, Z. M.
   Zhou, F.
   Zhuang, H. L.
   Zhukov, V.
   Zichichi, A.
   Zimmermann, N.
   Zuccon, P.
   Zurbach, C.
CA AMS Collaboration
TI High Statistics Measurement of the Positron Fraction in Primary Cosmic
   Rays of 0.5-500 GeV with the Alpha Magnetic Spectrometer on the
   International Space Station
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID TIME-OF-FLIGHT; AMS RICH DETECTOR; FAST TRIGGER; DARK-MATTER;
   IDENTIFICATION; ELECTRONS; PROTOTYPE; SPECTRUM; MODELS; ORIGIN
AB A precision measurement by AMS of the positron fraction in primary cosmic rays in the energy range from 0.5 to 500 GeV based on 10.9 million positron and electron events is presented. This measurement extends the energy range of our previous observation and increases its precision. The new results show, for the first time, that above similar to 200 GeV the positron fraction no longer exhibits an increase with energy.
C1 [Bachlechner, A.; Beischer, B.; Chung, C. H.; Gast, H.; Kirn, Th.; Li, Q.; Luebelsmeyer, K.; Mueller, M.; Obermeier, A.; Schael, S.; von Dratzig, A. Schulz; Schwering, G.; Siedenburg, T.; Wienkenhoever, J.; Xie, M.; Zhukov, V.; Zimmermann, N.] Rhein Westfal TH Aachen, Inst Phys, D-52056 Aachen, Germany.
   [Bachlechner, A.; Beischer, B.; Chung, C. H.; Gast, H.; Kirn, Th.; Li, Q.; Luebelsmeyer, K.; Mueller, M.; Obermeier, A.; Schael, S.; von Dratzig, A. Schulz; Schwering, G.; Siedenburg, T.; Wienkenhoever, J.; Xie, M.; Zhukov, V.; Zimmermann, N.] Rhein Westfal TH Aachen, JARA FAME, D-52056 Aachen, Germany.
   [Demirkoez, M. B.; Postaci, E.; Tuerkoglu, C.] METU, Dept Phys, TR-06800 Ankara, Turkey.
   [Basara, L.; Caroff, S.; Coignet, G.; Feng, J.; Fiasson, A.; Goy, C.; Kossakowski, R.; Poireau, V.; Putze, A.; Rosier-Lees, S.; Tao, L.; Vecchi, M.; Vialle, J. P.] CNRS, IN2P3, LAPP, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France.
   [Basara, L.; Caroff, S.; Coignet, G.; Feng, J.; Fiasson, A.; Goy, C.; Kossakowski, R.; Poireau, V.; Putze, A.; Rosier-Lees, S.; Tao, L.; Vecchi, M.; Vialle, J. P.] Univ Savoie, F-74941 Annecy Le Vieux, France.
   [Li, W.; Shan, B. S.; Shan, Y. H.; Zheng, Z. M.] Beihang Univ, BUAA, Beijing 100191, Peoples R China.
   [Dai, M.; Wang, Q. L.; Yu, Y. J.] Chinese Acad Sci, IEE, Beijing 100080, Peoples R China.
   [Cheng, G. M.; Chen, H. S.; Li, Z. H.; Lu, Y. S.; Tang, X. W.; Tang, Z. C.; Xu, W.; Yan, Q.; Yang, M.; Yu, Z. Q.; Zhuang, H. L.] Chinese Acad Sci, IHEP, Beijing 100039, Peoples R China.
   [Cindolo, F.; Contin, A.; Guandalini, C.; Laurenti, G.; Levi, G.; Lolli, M.; Masi, N.; Massera, F.; Palmonari, F.; Pilastrini, R.; Quadrani, L.; Sbarra, C.; Zichichi, A.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy.
   [Cindolo, F.; Contin, A.; Guandalini, C.; Laurenti, G.; Levi, G.; Lolli, M.; Masi, N.; Massera, F.; Palmonari, F.; Pilastrini, R.; Quadrani, L.; Sbarra, C.; Zichichi, A.] Univ Bologna, I-40126 Bologna, Italy.
   [Becker, U.; Behlmann, M.; Burger, J.; Cai, X. D.; Capell, M.; Carosi, G.; Chen, A. I.; Chen, H.; Choumilov, E.; Choutko, V.; Eline, A.; Eppling, F. J.; Fisher, P.; Galaktionov, Y.; Goglov, P.; Heil, M.; Henning, R.; Hsieh, T. H.; Kounina, O.; Kounine, A.; Koutsenko, V.; Krafczyk, M. S.; Lebedev, A.; Li, Q.; Monreal, B.; Plyaskin, V.; Rozhkov, A.; Rybka, G.; Shi, X. Y.; Sun, W.; Sun, W. H.; Ting, Samuel C. C.; Ting, S. M.; Vaurynovich, S.; Wang, X.; Weng, Z. L.; Xie, M.; Xu, W.; Zhou, F.; Zuccon, P.] MIT, Cambridge, MA 02139 USA.
   [Chang, Y. H.; Chou, H. Y.; Gillard, W.; Haino, S.; Hoffman, J.] NCU, Taoyuan 32054, Taiwan.
   [Sagdeev, R.] Univ Maryland, East West Ctr Space Sci, College Pk, MD 20742 USA.
   [Malinin, A.; Seo, E. S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
   [Huh, C.; Jang, W. Y.; Kim, G. N.; Kim, K. S.; Son, D.] Kyungpook Natl Univ, CHEP, Taegu 702701, South Korea.
   [Castellini, G.] CNR, IROE, I-50125 Florence, Italy.
   [Barrin, L.; Gallucci, G.; Graziani, M.; La Vacca, G.; Rossi, L.] CERN, European Org Nucl Res, CH-1211 Geneva 23, Switzerland.
   [Azzarello, P.; Bourquin, M.; Cadoux, F.; Haas, D.; Habiby, M.; Leluc, C.; Li, Y.; Paniccia, M.; Pohl, M.; Rapin, D.; Saouter, P.] Univ Geneva, DPNC, CH-1211 Geneva 4, Switzerland.
   [Barrau, A.; Bonnivard, V.; Derome, L.; Ghelfi, A.; Maurin, D.; Ricol, J. S.; Tomassetti, N.] Univ Grenoble Alpes, LPSC, F-38026 Grenoble, France.
   [Guo, K. H.; He, Z. H.; Huang, Z. C.; Li, T. X.; Lv, S. S.; Mo, D. C.; Ni, J. Q.; Qi, X. M.; Tang, C. P.; Wang, Z. X.; Xu, N. S.; Zhang, M. T.; Zhang, X. B.; Zhang, Z.] SYSU, Guangzhou 510275, Guangdong, Peoples R China.
   [Bindi, V.; Consolandi, C.; Corti, C.; von Doetinchem, P.; Pereira, R.; Whitman, K.] Univ Hawaii, Phys & Astron Dept, Honolulu, HI 96822 USA.
   [Bollweg, K.; Clark, C.; Martin, T.; Mott, P.; Urban, T.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
   [Bollweg, K.; Clark, C.; Martin, T.; Mott, P.; Urban, T.] Jacobs Sverdrup, Houston, TX 77058 USA.
   [Attig, N.; Lippert, T.; Schmidt, S. M.] Julich Supercomp Ctr, D-52425 Julich, Germany.
   [Attig, N.; Lippert, T.; Schmidt, S. M.] Res Ctr Julich, JARA FAME, D-52425 Julich, Germany.
   [Andeen, K.; de Boer, W.; Gebauer, I.; Heil, M.; Kunz, S.; Nikonov, N.; Schuckardt, D.; Vagelli, V.; Zeissler, S.] KIT, Inst Expt Kernphys, D-76128 Karlsruhe, Germany.
   [Clavero, R.; Garcia-Lopez, R.; Tescaro, D.] IAC, E-38205 Tenerife, Spain.
   [Arruda, L.; Barao, F.; Nunes, P.; Orcinha, M.; Pereira, R.] LIP, Lab Instrumentacao & Fis Expt Particulas, P-1000 Lisbon, Portugal.
   [Han, K. C.; Jinchi, H.] NCSIST, Taoyuan 325, Taiwan.
   [Aguilar, M.; Berdugo, J.; Casaus, J.; Cernuda, I.; Delgado, C.; Diaz, C.; Garcia, B.; Giovacchini, F.; Mana, C.; Marin, J.; Martinez, G.; Oliva, A.; Palomares, C.; Rodriguez, I.; Velasco, M.; Xia, X.] CIEMAT, Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain.
   [Grabski, V.; Menchaca-Rocha, A.] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 01000, DF, Mexico.
   [Volpini, G.] Ist Nazl Fis Nucl, Sez Milano, I-20090 Milan, Italy.
   [Volpini, G.] Univ Milan, I-20090 Milan, Italy.
   [Boella, G.; Boschini, M. J.; Della Torre, S.; Gervasi, M.; Grandi, D.; La Vacca, G.; Pensotti, S.; Rancoita, P. G.; Rozza, D.; Tacconi, M.] Ist Nazl Fis Nucl, Sez Milano Bicocca, I-20126 Milan, Italy.
   [Boella, G.; Gervasi, M.; Pensotti, S.; Tacconi, M.] Univ Milano Bicocca, I-20126 Milan, Italy.
   [Zurbach, C.] CNRS, IN2P3, LUPM, F-34095 Montpellier, France.
   [Zurbach, C.] Univ Montpellier 2, F-34095 Montpellier, France.
   [Gong, J.; Li, J. Q.; Li, Q.; Liu, H.; Luo, J. Z.; Meng, Q.; Shi, J. Y.; Wu, H.; Xiong, R. Q.; Yi, H.; Zhang, J. H.] Southeast Univ, SEU, Nanjing 210096, Jiangsu, Peoples R China.
   [Chikanian, A.; Finch, E.; Majka, R.; Sandweiss, J.] Yale Univ, Phys Dept, New Haven, CT 06520 USA.
   [Accardo, L.; Aisa, D.; Alpat, B.; Alvino, A.; Ambrosi, G.; Azzarello, P.; Bazo, J.; Bertucci, B.; Bizzaglia, S.; Bizzarri, M.; Borsini, S.; Cascioli, V.; Cerreta, D.; Di Masso, L.; Duranti, M.; D'Urso, D.; Farnesini, L.; Fiandrini, E.; Graziani, M.; Ionica, M.; Laudi, E.; Nozzoli, F.; Papi, A.; Pauluzzi, M.; Piluso, A.; Pizzolotto, C.; Scolieri, G.; Vitale, V.] Ist Nazl Fis Nucl, Sez Perugia, I-06100 Perugia, Italy.
   [Aisa, D.; Bertucci, B.; Bizzarri, M.; Cerreta, D.; Di Masso, L.; Fiandrini, E.; Laudi, E.; Pauluzzi, M.; Piluso, A.] Univ Perugia, I-06100 Perugia, Italy.
   [Bigongiari, G.; Cervelli, F.; Di Falco, S.; Gallucci, G.; Guerri, I.; Incagli, M.; Lomtadze, T.; Morescalchi, L.; Pedreschi, E.; Pilo, F.; Spinella, F.; Vannini, C.] Ist Nazl Fis Nucl, Sez Pisa, I-56100 Pisa, Italy.
   [Bigongiari, G.; Guerri, I.] Univ Pisa, I-56100 Pisa, Italy.
   [Basara, L.; Battiston, R.; Coste, B.; Dimiccoli, F.; Kanishev, K.; Lazzizzera, I.; Lu, M. J.] Ist Nazl Fis Nucl, TIFPA, I-38123 Povo, Trento, Italy.
   [Basara, L.; Battiston, R.; Coste, B.; Dimiccoli, F.; Kanishev, K.; Lazzizzera, I.; Lu, M. J.] Univ Trento, I-38123 Povo, Trento, Italy.
   [Bartoloni, A.; Borgia, B.; Lipari, P.; Spada, F.; Valente, E.] Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy.
   [Borgia, B.; Valente, E.] Univ Roma La Sapienza, I-00185 Rome, Italy.
   [Chae, M. J.; Lim, S.; Yang, J.] Ewha Womans Univ, Dept Phys, Seoul 120750, South Korea.
   [Cheng, L.; Cui, Z.; Du, W. J.; Luo, F.; Wang, L. Q.; Xin, G. M.] Shandong Univ, SDU, Jinan 250100, Shandong, Peoples R China.
   [Shi, Y. M.; Wang, R. S.; Xie, S.; Ye, Q. H.] Shanghai Jiao Tong Univ, SJTU, Shanghai 200030, Peoples R China.
   [Fan, Y. Y.; Haino, S.; Lee, H. T.; Lee, S. C.; Li, H. L.; Li, Z. Y.; Lin, C. H.; Liu, D.; Wu, K. Y.] Acad Sinica, Inst Phys, Taipei 11529, Taiwan.
   [Battarbee, M.; Eronen, T.; Torsti, J.; Valtonen, E.] Univ Turku, Dept Phys & Astron, Space Res Lab, FI-20014 Turku, Finland.
   [Fan, Y. Y.] Xi An Jiao Tong Univ, Xian 710049, Peoples R China.
   [Feng, J.; Li, Y.; Li, Z. Y.] SYSU, Guangzhou 510275, Guangdong, Peoples R China.
   [Li, H. L.; Xia, X.] Shandong Univ, SDU, Jinan, Shandong, Peoples R China.
   [Henning, R.] HIT, Harbin 150001, Peoples R China.
   [Lu, M. J.] USTC, Hefei 230026, Peoples R China.
   [Morescalchi, L.] Univ Siena, I-53100 Siena, Italy.
   [Shi, X. Y.] Beijing Normal Univ, Beijing 100875, Peoples R China.
   [Sun, W. H.] Southeast Univ, SEU, Nanjing 210096, Jiangsu, Peoples R China.
RP Accardo, L (reprint author), Ist Nazl Fis Nucl, Sez Perugia, I-06100 Perugia, Italy.
RI Pizzolotto, Cecilia/G-5821-2013; Orcinha, Miguel/O-2362-2016; Barao,
   Fernando/O-2357-2016; Paniccia, Mercedes/A-4519-2017; Arruda,
   Luisa/I-2403-2013; Lazzizzera, Ignazio/E-9678-2015; Berdugo,
   Javier/A-2858-2015; Tomassetti, Nicola/K-2380-2016; Demirkoz,
   Bilge/C-8179-2014; Masi, Nicolo/G-7911-2016; Delgado,
   Carlos/K-7587-2014; Vecchi, Manuela/J-9180-2014; alpat, ali
   behcet/G-6290-2013; Rancoita, Pier Giorgio/J-9896-2015; Zuccon,
   Paolo/I-7736-2012; Ye, Qinghao/O-5630-2015; Fiandrini,
   Emanuele/C-4549-2008; Palomares, Carmen/H-7783-2015; Duranti,
   Matteo/I-7691-2013
OI Morescalchi, Luca/0000-0002-7819-8139; Bertucci,
   Bruna/0000-0001-7584-293X; Graziani, Maura/0000-0001-7570-2048; Vagelli,
   Valerio/0000-0002-4495-9331; La Vacca, Giuseppe/0000-0002-2168-9447;
   Seo, Eun-Suk/0000-0001-8682-805X; Ambrosi, Giovanni/0000-0001-6977-9559;
   Castellini, Guido/0000-0002-0177-0643; Quadrani,
   Lucio/0000-0003-4830-0259; LI, Qiang/0000-0002-2870-4101; Gallucci,
   Giovanni/0000-0003-3554-9733; Basara, Laurent/0000-0002-5726-9954;
   Corti, Claudio/0000-0001-9127-7133; Pizzolotto,
   Cecilia/0000-0003-0200-2408; Orcinha, Miguel/0000-0003-1874-2144; Barao,
   Fernando/0000-0002-8346-9941; Paniccia, Mercedes/0000-0001-8482-2703;
   Arruda, Luisa/0000-0001-6720-6933; Tacconi, Mauro/0000-0002-9344-6305;
   Bigongiari, Gabriele/0000-0003-3691-0826; Rozza,
   Davide/0000-0002-7378-6353; GILLARD, William/0000-0003-4744-9748;
   Lazzizzera, Ignazio/0000-0001-5092-7531; Berdugo,
   Javier/0000-0002-7911-8532; Tomassetti, Nicola/0000-0002-0856-9299;
   Masi, Nicolo/0000-0002-3729-7608; Delgado, Carlos/0000-0002-7014-4101;
   alpat, ali behcet/0000-0002-0116-1506; Rancoita, Pier
   Giorgio/0000-0002-1990-4283; Zuccon, Paolo/0000-0002-2728-0167;
   Palomares, Carmen/0000-0003-4374-9065; Duranti,
   Matteo/0000-0003-0980-6425
FU NASA; U.S. DOE; M.I.T., School of Science; CAS, China; NNSF, China;
   MOST, China; NLAA, China; provincial government of Shandong, China;
   provincial government of Jiangsu, China; provincial government of
   Guangdong, China; CNRS, France; IN2P3, France; CNES, France; Enigmass,
   France; ANR, France; CIEMAT, Spain; CDTI, Spain; SEIDI-MINECO, Spain;
   CPAN, Spain; Swiss National Science Foundation (SNSF); Academia Sinica;
   National Science Council (NSC); CERN; ESA
FX We thank former NASA Administrator Daniel S. Goldin for his dedication
   to the legacy of the ISS as a scientific laboratory and his decision for
   NASA to fly AMS as a DOE payload. We also acknowledge the continuous
   support of the NASA leadership including Charles Bolden, William
   Gerstenmeier, and Mark Sistilli. AMS is a U.S. DOE sponsored
   international collaboration. We are grateful for the support of Jim
   Siegrist, Michael Salamon, Dennis Kovar, Robin Staffin, Saul Gonzalez,
   and John O'Fallon of the DOE. We also acknowledge the continuous support
   from M.I.T. and its School of Science, Michael Sipser, Marc Kastner,
   Ernest Moniz, Edmund Bertschinger, and Richard Milner. We acknowledge
   support from: CAS, NNSF, MOST, NLAA, and the provincial governments of
   Shandong, Jiangsu, and Guangdong, China; CNRS, IN2P3, CNES, Enigmass,
   and the ANR, France, and Bernard Accoyer, former President of the French
   National Assembly; DLR, P. Hintze, J. Trumper, and J. D. Woerner,
   Germany; INFN, E. Iarocci, R. Petronzio, and F. Ferroni, and ASI, S. De
   Julio, S. Vetrella, G. Bignami, and E. Saggese, Italy; CIEMAT, CDTI,
   SEIDI-MINECO, and CPAN, Spain; the Swiss National Science Foundation
   (SNSF), federal and cantonal authorities, Switzerland; and Academia
   Sinica and the National Science Council (NSC), former President of
   Academia Sinica Yuan-Tseh Lee and former Ministers of NSC, Chien-Jen
   Chen, Maw-Kuen Wu, and Luo-Chuan Lee, Taiwan. We gratefully acknowledge
   the strong support from CERN: Rolf-Dieter Heuer, Robert Aymar, Luciano
   Maiani, as well as Steve Meyers and Andrzej Siemko. From ESA, we thank
   Jean-Jacques Dordain, Simona Di Pippo, and Martin Zell for their
   support. We are grateful for important discussions with Barry Barish,
   Claude Canizares, James Cronin, Jonathan Ellis, Len Fisk, Sheldon
   Glashow, Alan Guth, Neal Lane, Steve Olsen, Alvaro de Rujula, George
   Smoot, Jian Song, Evgeny Velikhov, Steven Weinberg, Frank Wilczek, and
   Cunhao Zhang. We are most grateful for the strong support of the flight
   control teams at Johnson Space Center, Houston, and Marshall Space
   Flight Center, Huntsville, which has allowed AMS to operate continuously
   on the ISS for over three years.
NR 60
TC 142
Z9 148
U1 16
U2 95
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 18
PY 2014
VL 113
IS 12
AR 121101
DI 10.1103/PhysRevLett.113.121101
PG 9
WC Physics, Multidisciplinary
SC Physics
GA AU7II
UT WOS:000345773700005
PM 25279616
ER

PT J
AU Aguilar, M
   Aisa, D
   Alvino, A
   Ambrosi, G
   Andeen, K
   Arruda, L
   Attig, N
   Azzarello, P
   Bachlechner, A
   Barao, F
   Barrau, A
   Barrin, L
   Bartoloni, A
   Basara, L
   Battarbee, M
   Battiston, R
   Bazo, J
   Becker, U
   Behlmann, M
   Beischer, B
   Berdugo, J
   Bertucci, B
   Bigongiari, G
   Bindi, V
   Bizzaglia, S
   Bizzarri, M
   Boella, G
   de Boer, W
   Bollweg, K
   Bonnivard, V
   Borgia, B
   Borsini, S
   Boschini, MJ
   Bourquin, M
   Burger, J
   Cadoux, F
   Cai, XD
   Capell, M
   Caroff, S
   Casaus, J
   Cascioli, V
   Castellini, G
   Cernuda, I
   Cervelli, F
   Chae, MJ
   Chang, YH
   Chen, AI
   Chen, H
   Cheng, GM
   Chen, HS
   Cheng, L
   Chikanian, A
   Chou, HY
   Choumilov, E
   Choutko, V
   Chung, CH
   Clark, C
   Clavero, R
   Coignet, G
   Consolandi, C
   Contin, A
   Corti, C
   Coste, B
   Cui, Z
   Dai, M
   Delgado, C
   Della Torre, S
   Demirkoz, MB
   Derome, L
   Di Falco, S
   Di Masso, L
   Dimiccoli, F
   Diaz, C
   von Doetinchem, P
   Du, WJ
   Duranti, M
   D'Urso, D
   Eline, A
   Eppling, FJ
   Eronen, T
   Fan, YY
   Farnesini, L
   Feng, J
   Fiandrini, E
   Fiasson, A
   Finch, E
   Fisher, P
   Galaktionov, Y
   Gallucci, G
   Garcia, B
   Garcia-Lopez, R
   Gast, H
   Gebauer, I
   Gervasi, M
   Ghelfi, A
   Gillard, W
   Giovacchini, F
   Goglov, P
   Gong, J
   Goy, C
   Grabski, V
   Grandi, D
   Graziani, M
   Guandalini, C
   Guerri, I
   Guo, KH
   Habiby, M
   Haino, S
   Han, KC
   He, ZH
   Heil, M
   Hoffman, J
   Hsieh, TH
   Huang, ZC
   Huh, C
   Incagli, M
   Ionica, M
   Jang, WY
   Jinchi, H
   Kanishev, K
   Kim, GN
   Kim, KS
   Kirn, T
   Kossakowski, R
   Kounina, O
   Kounine, A
   Koutsenko, V
   Krafczyk, MS
   Kunz, S
   La Vacca, G
   Laudi, E
   Laurenti, G
   Lazzizzera, I
   Lebedev, A
   Lee, HT
   Lee, SC
   Leluc, C
   Li, HL
   Li, JQ
   Li, Q
   Li, Q
   Li, TX
   Li, W
   Li, Y
   Li, ZH
   Li, ZY
   Lim, S
   Lin, CH
   Lipari, P
   Lippert, T
   Liu, D
   Liu, H
   Lomtadze, T
   Lu, MJ
   Lu, YS
   Luebelsmeyer, K
   Luo, F
   Luo, JZ
   Lv, SS
   Majka, R
   Malinin, A
   Mana, C
   Marin, J
   Martin, T
   Martinez, G
   Masi, N
   Maurin, D
   Menchaca-Rocha, A
   Meng, Q
   Mo, DC
   Morescalchi, L
   Mott, P
   Muller, M
   Ni, JQ
   Nikonov, N
   Nozzoli, F
   Nunes, P
   Obermeier, A
   Oliva, A
   Orcinha, M
   Palmonari, F
   Palomares, C
   Paniccia, M
   Papi, A
   Pedreschi, E
   Pensotti, S
   Pereira, R
   Pilo, F
   Piluso, A
   Pizzolotto, C
   Plyaskin, V
   Pohl, M
   Poireau, V
   Postaci, E
   Putze, A
   Quadrani, L
   Qi, XM
   Rancoita, PG
   Rapin, D
   Ricol, JS
   Rodriguez, I
   Rosier-Lees, S
   Rozhkov, A
   Rozza, D
   Sagdeev, R
   Sandweiss, J
   Saouter, P
   Sbarra, C
   Schael, S
   Schmidt, SM
   Schuckardt, D
   von Dratzig, AS
   Schwering, G
   Scolieri, G
   Seo, ES
   Shan, BS
   Shan, YH
   Shi, JY
   Shi, XY
   Shi, YM
   Siedenburg, T
   Son, D
   Spada, F
   Spinella, F
   Sun, W
   Sun, WH
   Tacconi, M
   Tang, CP
   Tang, XW
   Tang, ZC
   Tao, L
   Tescaro, D
   Ting, SCC
   Ting, SM
   Tomassetti, N
   Torsti, J
   Turkoglu, C
   Urban, T
   Vagelli, V
   Valente, E
   Vannini, C
   Valtonen, E
   Vaurynovich, S
   Vecchi, M
   Velasco, M
   Vialle, JP
   Wang, LQ
   Wang, QL
   Wang, RS
   Wang, X
   Wang, ZX
   Weng, ZL
   Whitman, K
   Wienkenhover, J
   Wu, H
   Xia, X
   Xie, M
   Xie, S
   Xiong, RQ
   Xin, GM
   Xu, NS
   Xu, W
   Yan, Q
   Yang, J
   Yang, M
   Ye, QH
   Yi, H
   Yu, YJ
   Yu, ZQ
   Zeissler, S
   Zhang, JH
   Zhang, MT
   Zhang, XB
   Zhang, Z
   Zheng, ZM
   Zhuang, HL
   Zhukov, V
   Zichichi, A
   Zimmermann, N
   Zuccon, P
   Zurbach, C
AF Aguilar, M.
   Aisa, D.
   Alvino, A.
   Ambrosi, G.
   Andeen, K.
   Arruda, L.
   Attig, N.
   Azzarello, P.
   Bachlechner, A.
   Barao, F.
   Barrau, A.
   Barrin, L.
   Bartoloni, A.
   Basara, L.
   Battarbee, M.
   Battiston, R.
   Bazo, J.
   Becker, U.
   Behlmann, M.
   Beischer, B.
   Berdugo, J.
   Bertucci, B.
   Bigongiari, G.
   Bindi, V.
   Bizzaglia, S.
   Bizzarri, M.
   Boella, G.
   de Boer, W.
   Bollweg, K.
   Bonnivard, V.
   Borgia, B.
   Borsini, S.
   Boschini, M. J.
   Bourquin, M.
   Burger, J.
   Cadoux, F.
   Cai, X. D.
   Capell, M.
   Caroff, S.
   Casaus, J.
   Cascioli, V.
   Castellini, G.
   Cernuda, I.
   Cervelli, F.
   Chae, M. J.
   Chang, Y. H.
   Chen, A. I.
   Chen, H.
   Cheng, G. M.
   Chen, H. S.
   Cheng, L.
   Chikanian, A.
   Chou, H. Y.
   Choumilov, E.
   Choutko, V.
   Chung, C. H.
   Clark, C.
   Clavero, R.
   Coignet, G.
   Consolandi, C.
   Contin, A.
   Corti, C.
   Coste, B.
   Cui, Z.
   Dai, M.
   Delgado, C.
   Della Torre, S.
   Demirkoez, M. B.
   Derome, L.
   Di Falco, S.
   Di Masso, L.
   Dimiccoli, F.
   Diaz, C.
   von Doetinchem, P.
   Du, W. J.
   Duranti, M.
   D'Urso, D.
   Eline, A.
   Eppling, F. J.
   Eronen, T.
   Fan, Y. Y.
   Farnesini, L.
   Feng, J.
   Fiandrini, E.
   Fiasson, A.
   Finch, E.
   Fisher, P.
   Galaktionov, Y.
   Gallucci, G.
   Garcia, B.
   Garcia-Lopez, R.
   Gast, H.
   Gebauer, I.
   Gervasi, M.
   Ghelfi, A.
   Gillard, W.
   Giovacchini, F.
   Goglov, P.
   Gong, J.
   Goy, C.
   Grabski, V.
   Grandi, D.
   Graziani, M.
   Guandalini, C.
   Guerri, I.
   Guo, K. H.
   Habiby, M.
   Haino, S.
   Han, K. C.
   He, Z. H.
   Heil, M.
   Hoffman, J.
   Hsieh, T. H.
   Huang, Z. C.
   Huh, C.
   Incagli, M.
   Ionica, M.
   Jang, W. Y.
   Jinchi, H.
   Kanishev, K.
   Kim, G. N.
   Kim, K. S.
   Kirn, Th.
   Kossakowski, R.
   Kounina, O.
   Kounine, A.
   Koutsenko, V.
   Krafczyk, M. S.
   Kunz, S.
   La Vacca, G.
   Laudi, E.
   Laurenti, G.
   Lazzizzera, I.
   Lebedev, A.
   Lee, H. T.
   Lee, S. C.
   Leluc, C.
   Li, H. L.
   Li, J. Q.
   Li, Q.
   Li, Q.
   Li, T. X.
   Li, W.
   Li, Y.
   Li, Z. H.
   Li, Z. Y.
   Lim, S.
   Lin, C. H.
   Lipari, P.
   Lippert, T.
   Liu, D.
   Liu, H.
   Lomtadze, T.
   Lu, M. J.
   Lu, Y. S.
   Luebelsmeyer, K.
   Luo, F.
   Luo, J. Z.
   Lv, S. S.
   Majka, R.
   Malinin, A.
   Mana, C.
   Marin, J.
   Martin, T.
   Martinez, G.
   Masi, N.
   Maurin, D.
   Menchaca-Rocha, A.
   Meng, Q.
   Mo, D. C.
   Morescalchi, L.
   Mott, P.
   Mueller, M.
   Ni, J. Q.
   Nikonov, N.
   Nozzoli, F.
   Nunes, P.
   Obermeier, A.
   Oliva, A.
   Orcinha, M.
   Palmonari, F.
   Palomares, C.
   Paniccia, M.
   Papi, A.
   Pedreschi, E.
   Pensotti, S.
   Pereira, R.
   Pilo, F.
   Piluso, A.
   Pizzolotto, C.
   Plyaskin, V.
   Pohl, M.
   Poireau, V.
   Postaci, E.
   Putze, A.
   Quadrani, L.
   Qi, X. M.
   Rancoita, P. G.
   Rapin, D.
   Ricol, J. S.
   Rodriguez, I.
   Rosier-Lees, S.
   Rozhkov, A.
   Rozza, D.
   Sagdeev, R.
   Sandweiss, J.
   Saouter, P.
   Sbarra, C.
   Schael, S.
   Schmidt, S. M.
   Schuckardt, D.
   von Dratzig, A. Schulz
   Schwering, G.
   Scolieri, G.
   Seo, E. S.
   Shan, B. S.
   Shan, Y. H.
   Shi, J. Y.
   Shi, X. Y.
   Shi, Y. M.
   Siedenburg, T.
   Son, D.
   Spada, F.
   Spinella, F.
   Sun, W.
   Sun, W. H.
   Tacconi, M.
   Tang, C. P.
   Tang, X. W.
   Tang, Z. C.
   Tao, L.
   Tescaro, D.
   Ting, Samuel C. C.
   Ting, S. M.
   Tomassetti, N.
   Torsti, J.
   Tuerkoglu, C.
   Urban, T.
   Vagelli, V.
   Valente, E.
   Vannini, C.
   Valtonen, E.
   Vaurynovich, S.
   Vecchi, M.
   Velasco, M.
   Vialle, J. P.
   Wang, L. Q.
   Wang, Q. L.
   Wang, R. S.
   Wang, X.
   Wang, Z. X.
   Weng, Z. L.
   Whitman, K.
   Wienkenhoever, J.
   Wu, H.
   Xia, X.
   Xie, M.
   Xie, S.
   Xiong, R. Q.
   Xin, G. M.
   Xu, N. S.
   Xu, W.
   Yan, Q.
   Yang, J.
   Yang, M.
   Ye, Q. H.
   Yi, H.
   Yu, Y. J.
   Yu, Z. Q.
   Zeissler, S.
   Zhang, J. H.
   Zhang, M. T.
   Zhang, X. B.
   Zhang, Z.
   Zheng, Z. M.
   Zhuang, H. L.
   Zhukov, V.
   Zichichi, A.
   Zimmermann, N.
   Zuccon, P.
   Zurbach, C.
CA AMS Collaboration
TI Electron and Positron Fluxes in Primary Cosmic Rays Measured with the
   Alpha Magnetic Spectrometer on the International Space Station
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID AMS-02; SPECTRA; MODELS; ORIGIN; EXCESS
AB Precision measurements by the Alpha Magnetic Spectrometer on the International Space Station of the primary cosmic-ray electron flux in the range 0.5 to 700 GeV and the positron flux in the range 0.5 to 500 GeV are presented. The electron flux and the positron flux each require a description beyond a single power-law spectrum. Both the electron flux and the positron flux change their behavior at similar to 30 GeV but the fluxes are significantly different in their magnitude and energy dependence. Between 20 and 200 GeV the positron spectral index is significantly harder than the electron spectral index. The determination of the differing behavior of the spectral indices versus energy is a new observation and provides important information on the origins of cosmic-ray electrons and positrons.
C1 [Bachlechner, A.; Beischer, B.; Chung, C. H.; Gast, H.; Kirn, Th.; Luebelsmeyer, K.; Mueller, M.; Obermeier, A.; Schael, S.; von Dratzig, A. Schulz; Schwering, G.; Siedenburg, T.; Wienkenhoever, J.; Zhukov, V.; Zimmermann, N.] Rhein Westfal TH Aachen, Inst Phys, D-52056 Aachen, Germany.
   [Bachlechner, A.; Beischer, B.; Chung, C. H.; Gast, H.; Kirn, Th.; Luebelsmeyer, K.; Mueller, M.; Obermeier, A.; Schael, S.; von Dratzig, A. Schulz; Schwering, G.; Siedenburg, T.; Wienkenhoever, J.; Zhukov, V.; Zimmermann, N.] Rhein Westfal TH Aachen, JARA FAME, D-52056 Aachen, Germany.
   [Demirkoez, M. B.; Postaci, E.; Tuerkoglu, C.] METU, Dept Phys, TR-06800 Ankara, Turkey.
   [Basara, L.; Caroff, S.; Coignet, G.; Feng, J.; Fiasson, A.; Goy, C.; Kossakowski, R.; Poireau, V.; Putze, A.; Rosier-Lees, S.; Tao, L.; Vecchi, M.; Vialle, J. P.] CNRS, IN2P3, LAPP, F-74941 Annecy Le Vieux, France.
   [Basara, L.; Caroff, S.; Coignet, G.; Feng, J.; Fiasson, A.; Goy, C.; Kossakowski, R.; Poireau, V.; Putze, A.; Rosier-Lees, S.; Tao, L.; Vecchi, M.; Vialle, J. P.] Univ Savoie, F-74941 Annecy Le Vieux, France.
   [Li, W.; Shan, B. S.; Shan, Y. H.; Zheng, Z. M.] Beihang Univ BUAA, Beijing 100191, Peoples R China.
   [Dai, M.; Wang, Q. L.; Yu, Y. J.] Chinese Acad Sci, IEE, Beijing 100080, Peoples R China.
   [Cheng, G. M.; Chen, H. S.; Li, Z. H.; Lu, Y. S.; Tang, X. W.; Tang, Z. C.; Xu, W.; Yan, Q.; Yang, M.; Yu, Z. Q.; Zhuang, H. L.] Chinese Acad Sci, IHEP, Beijing 100039, Peoples R China.
   [Contin, A.; Guandalini, C.; Laurenti, G.; Masi, N.; Palmonari, F.; Quadrani, L.; Sbarra, C.; Zichichi, A.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy.
   [Contin, A.; Guandalini, C.; Laurenti, G.; Masi, N.; Palmonari, F.; Quadrani, L.; Sbarra, C.; Zichichi, A.] Univ Bologna, I-40126 Bologna, Italy.
   [Becker, U.; Behlmann, M.; Burger, J.; Cai, X. D.; Capell, M.; Chen, A. I.; Chen, H.; Choumilov, E.; Choutko, V.; Eline, A.; Eppling, F. J.; Fisher, P.; Galaktionov, Y.; Goglov, P.; Heil, M.; Hsieh, T. H.; Kounina, O.; Kounine, A.; Koutsenko, V.; Krafczyk, M. S.; Lebedev, A.; Li, Q.; Plyaskin, V.; Rozhkov, A.; Shi, X. Y.; Sun, W.; Sun, W. H.; Ting, Samuel C. C.; Ting, S. M.; Vaurynovich, S.; Wang, X.; Weng, Z. L.; Xie, M.; Xu, W.; Zuccon, P.] MIT, Cambridge, MA 02139 USA.
   [Chang, Y. H.; Chou, H. Y.; Gillard, W.; Haino, S.; Hoffman, J.] Natl Cent Univ, Taoyuan 32054, Taiwan.
   [Sagdeev, R.] Univ Maryland, East West Ctr Space Sci, College Pk, MD 20742 USA.
   [Malinin, A.; Seo, E. S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
   [Huh, C.; Jang, W. Y.; Kim, G. N.; Kim, K. S.; Son, D.] Kyungpook Natl Univ, CHEP, Taegu 702701, South Korea.
   [Castellini, G.] CNR, IROE, I-50125 Florence, Italy.
   [Barrin, L.; Gallucci, G.; Graziani, M.; La Vacca, G.] CERN, European Org Nucl Res, CH-1211 Geneva 23, Switzerland.
   [Azzarello, P.; Bourquin, M.; Cadoux, F.; Habiby, M.; Leluc, C.; Li, Y.; Paniccia, M.; Pohl, M.; Rapin, D.; Saouter, P.] Univ Geneva, DPNC, CH-1211 Geneva 4, Switzerland.
   [Barrau, A.; Bonnivard, V.; Derome, L.; Ghelfi, A.; Maurin, D.; Ricol, J. S.; Tomassetti, N.] Univ Grenoble Alpes, LPSC, CNRS, IN2P3, F-38026 Grenoble, France.
   [Guo, K. H.; He, Z. H.; Huang, Z. C.; Li, T. X.; Lv, S. S.; Mo, D. C.; Ni, J. Q.; Qi, X. M.; Tang, C. P.; Wang, Z. X.; Xu, N. S.; Zhang, M. T.; Zhang, X. B.; Zhang, Z.] SYSU, Guangzhou 510275, Guangdong, Peoples R China.
   [Bindi, V.; Consolandi, C.; Corti, C.; von Doetinchem, P.; Pereira, R.; Whitman, K.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA.
   [Bollweg, K.; Clark, C.; Martin, T.; Mott, P.; Urban, T.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
   [Bollweg, K.; Clark, C.; Martin, T.; Mott, P.; Urban, T.] Jacobs Sverdrup, Houston, TX 77058 USA.
   [Attig, N.; Lippert, T.; Schmidt, S. M.] Julich Supercomp Ctr, D-52425 Julich, Germany.
   [Attig, N.; Lippert, T.; Schmidt, S. M.] Res Ctr Julich, JARA FAME, D-52425 Julich, Germany.
   [Andeen, K.; de Boer, W.; Gebauer, I.; Heil, M.; Kunz, S.; Nikonov, N.; Schuckardt, D.; Vagelli, V.; Zeissler, S.] Karlsruhe Inst Technol, Inst Expt Kernphys, D-76128 Karlsruhe, Germany.
   [Clavero, R.; Garcia-Lopez, R.; Tescaro, D.] IAC, E-38205 Tenerife, Spain.
   [Arruda, L.; Barao, F.; Nunes, P.; Orcinha, M.; Pereira, R.] LIP, Lab Instrumentacao & Fis Expt Particulas, P-1000 Lisbon, Portugal.
   [Han, K. C.; Jinchi, H.] NCSIST, Taoyuan 325, Taiwan.
   [Aguilar, M.; Berdugo, J.; Casaus, J.; Cernuda, I.; Delgado, C.; Diaz, C.; Garcia, B.; Giovacchini, F.; Mana, C.; Marin, J.; Martinez, G.; Oliva, A.; Palomares, C.; Rodriguez, I.; Velasco, M.; Xia, X.] Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid, Spain.
   [Grabski, V.; Menchaca-Rocha, A.] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 01000, DF, Mexico.
   [Boella, G.; Boschini, M. J.; Della Torre, S.; Gervasi, M.; Grandi, D.; La Vacca, G.; Pensotti, S.; Rancoita, P. G.; Rozza, D.; Tacconi, M.] Ist Nazl Fis Nucl, Sez Milano Bicocca, I-20126 Milan, Italy.
   [Boella, G.; Gervasi, M.; Pensotti, S.; Tacconi, M.] Univ Milano Bicocca, I-20126 Milan, Italy.
   [Zurbach, C.] CNRS, IN2P3, LUPM, F-34095 Montpellier, France.
   [Zurbach, C.] Univ Montpellier 2, F-34095 Montpellier, France.
   [Gong, J.; Li, J. Q.; Li, Q.; Liu, H.; Luo, J. Z.; Meng, Q.; Shi, J. Y.; Wu, H.; Xiong, R. Q.; Yi, H.; Zhang, J. H.] Southeast Univ, SEU, Nanjing 210096, Jiangsu, Peoples R China.
   [Chikanian, A.; Finch, E.; Majka, R.; Sandweiss, J.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
   [Aisa, D.; Alvino, A.; Ambrosi, G.; Azzarello, P.; Bazo, J.; Bertucci, B.; Bizzaglia, S.; Bizzarri, M.; Borsini, S.; Cascioli, V.; Di Masso, L.; Duranti, M.; D'Urso, D.; Farnesini, L.; Fiandrini, E.; Graziani, M.; Ionica, M.; Laudi, E.; Nozzoli, F.; Papi, A.; Piluso, A.; Pizzolotto, C.; Scolieri, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06100 Perugia, Italy.
   [Aisa, D.; Bertucci, B.; Bizzarri, M.; Di Masso, L.; Fiandrini, E.; Laudi, E.; Papi, A.; Piluso, A.] Univ Perugia, I-06100 Perugia, Italy.
   [Bigongiari, G.; Cervelli, F.; Di Falco, S.; Gallucci, G.; Guerri, I.; Incagli, M.; Lomtadze, T.; Morescalchi, L.; Pedreschi, E.; Pilo, F.; Spinella, F.; Vannini, C.] Ist Nazl Fis Nucl, Sez Pisa, I-56100 Pisa, Italy.
   [Bigongiari, G.; Guerri, I.] Univ Pisa, I-56100 Pisa, Italy.
   [Basara, L.; Battiston, R.; Coste, B.; Dimiccoli, F.; Kanishev, K.; Lazzizzera, I.; Lu, M. J.] Ist Nazl Fis Nucl, TIFPA, I-38123 Povo, Trento, Italy.
   [Basara, L.; Battiston, R.; Coste, B.; Dimiccoli, F.; Kanishev, K.; Lazzizzera, I.; Lu, M. J.] Univ Trento, I-38123 Povo, Trento, Italy.
   [Bartoloni, A.; Borgia, B.; Lipari, P.; Spada, F.; Valente, E.] Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy.
   [Borgia, B.; Valente, E.] Univ Roma La Sapienza, I-00185 Rome, Italy.
   [Chae, M. J.; Lim, S.; Yang, J.] Ewha Womans Univ, Dept Phys, Seoul 120750, South Korea.
   [Cheng, L.; Cui, Z.; Du, W. J.; Luo, F.; Wang, L. Q.; Xin, G. M.] Shandong Univ, SDU, Jinan 250100, Shandong, Peoples R China.
   [Shi, Y. M.; Wang, R. S.; Xie, S.; Ye, Q. H.] Shanghai Jiao Tong Univ, Shanghai 200030, Peoples R China.
   [Fan, Y. Y.; Haino, S.; Lee, H. T.; Lee, S. C.; Li, H. L.; Li, Z. Y.; Lin, C. H.; Liu, D.] Acad Sinica, Inst Phys, Taipei 11529, Taiwan.
   [Battarbee, M.; Eronen, T.; Torsti, J.; Valtonen, E.] Univ Turku, Dept Phys & Astron, Space Res Lab, FI-20014 Turku, Finland.
   [Battiston, R.] ASI, I-00133 Rome, Italy.
   [Fan, Y. Y.] Xi An Jiao Tong Univ, Xian 710049, Peoples R China.
   [Feng, J.; Li, Y.; Li, Z. Y.] SYSU, Guangzhou 510275, Guangdong, Peoples R China.
   [Li, H. L.] Shandong Univ, SDU, Jinan 250100, Shandong, Peoples R China.
   [Xie, M.] Harbin Inst Technol, Harbin 150001, Peoples R China.
   [Lu, M. J.] USTC, Hefei 230026, Peoples R China.
   [Morescalchi, L.] Univ Siena, I-53100 Siena, Italy.
   [Shi, X. Y.] Beijing Normal Univ, Beijing 100875, Peoples R China.
   [Sun, W. H.] Southeast Univ, SEU, Nanjing 210096, Jiangsu, Peoples R China.
RP Aguilar, M (reprint author), Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid, Spain.
RI Demirkoz, Bilge/C-8179-2014; Lazzizzera, Ignazio/E-9678-2015; Delgado,
   Carlos/K-7587-2014; Vecchi, Manuela/J-9180-2014; Rancoita, Pier
   Giorgio/J-9896-2015; Zuccon, Paolo/I-7736-2012; Ye, Qinghao/O-5630-2015;
   Fiandrini, Emanuele/C-4549-2008; Palomares, Carmen/H-7783-2015; Duranti,
   Matteo/I-7691-2013; Tomassetti, Nicola/K-2380-2016; Masi,
   Nicolo/G-7911-2016; Berdugo, Javier/A-2858-2015; Pizzolotto,
   Cecilia/G-5821-2013; Orcinha, Miguel/O-2362-2016; Barao,
   Fernando/O-2357-2016; Paniccia, Mercedes/A-4519-2017; Arruda,
   Luisa/I-2403-2013; 
OI Lazzizzera, Ignazio/0000-0001-5092-7531; Delgado,
   Carlos/0000-0002-7014-4101; Rancoita, Pier Giorgio/0000-0002-1990-4283;
   Zuccon, Paolo/0000-0002-2728-0167; Palomares,
   Carmen/0000-0003-4374-9065; Duranti, Matteo/0000-0003-0980-6425;
   Tomassetti, Nicola/0000-0002-0856-9299; Masi,
   Nicolo/0000-0002-3729-7608; Berdugo, Javier/0000-0002-7911-8532; Basara,
   Laurent/0000-0002-5726-9954; Corti, Claudio/0000-0001-9127-7133;
   Morescalchi, Luca/0000-0002-7819-8139; Bertucci,
   Bruna/0000-0001-7584-293X; Graziani, Maura/0000-0001-7570-2048; Vagelli,
   Valerio/0000-0002-4495-9331; La Vacca, Giuseppe/0000-0002-2168-9447;
   Castellini, Guido/0000-0002-0177-0643; Rozza,
   Davide/0000-0002-7378-6353; Bigongiari, Gabriele/0000-0003-3691-0826;
   GILLARD, William/0000-0003-4744-9748; Quadrani,
   Lucio/0000-0003-4830-0259; LI, Qiang/0000-0002-2870-4101; Gallucci,
   Giovanni/0000-0003-3554-9733; Pizzolotto, Cecilia/0000-0003-0200-2408;
   Orcinha, Miguel/0000-0003-1874-2144; Barao,
   Fernando/0000-0002-8346-9941; Paniccia, Mercedes/0000-0001-8482-2703; ,
   /0000-0002-8402-3116; Nozzoli, Francesco/0000-0002-4355-7947; Tacconi,
   Mauro/0000-0002-9344-6305; Arruda, Luisa/0000-0001-6720-6933; Ambrosi,
   Giovanni/0000-0001-6977-9559; Seo, Eun-Suk/0000-0001-8682-805X
FU NASA; MIT, School of Science; CAS, China; NNSF, China; MOST, China;
   NLAA, China; provincial government of Shandong, China; provincial
   government of Jiangsu, China; provincial government of Guangdong, China;
   CNRS, France; IN2P3, France; CNES, France; Enigmass, France; ANR,
   France; DLR, Germany; INFN, Italy; ASI, Italy; CIEMAT, Spain; CDTI,
   Spain; SEIDI-MINECO, Spain; CPAN, Spain; Swiss National Science
   Foundation (SNSF), Switzerland; Academia Sinica; National Science
   Council (NSC); CERN; ESA; ASI Science Data Center (ASDC) [C/011/11/1];
   Centre national d'etudes spatiales, CNES; Deutsches Zentrum fur Luft-
   und Raumfahrt, DLR; JARA-HPC [JARA0052]; Turkish Atomic Energy
   Authority, TAEK; National Natural Science Foundation of China; Italian
   Space Agency, ASI [ASI-INFN I/002/13/0]; Ministry of Science and
   Technology; CHEP, Kyungpook National University [NRF-2009-0080142,
   NRF-2012-010226]; SEIDI; CPAN; Consejo Nacional de Ciencia y Tecnologia,
   CONACYT; China Scholarship Council;  [NRF-2013-004883]
FX We thank former NASA Administrator Daniel S. Goldin for his dedication
   to the legacy of the ISS as a scientific laboratory and his decision for
   NASA to fly AMS as a DOE payload. We also acknowledge the support of the
   NASA leadership including Charles Bolden and William Gerstenmeier. We
   are grateful for the support of Jim Siegrist and Michael Salamon of the
   DOE. We also acknowledge the continuous support from MIT and its School
   of Science, Michael Sipser, Marc Kastner, Ernest Moniz, and Richard
   Milner. We acknowledge support from CAS, NNSF, MOST, NLAA, and the
   provincial governments of Shandong, Jiangsu, and Guangdong, China; CNRS,
   IN2P3, CNES, Enigmass, and the ANR, France; J. Trumper, J. D. Woerner,
   and DLR, Germany; INFN and ASI, Italy; CIEMAT, CDTI, SEIDI-MINECO, and
   CPAN, Spain; the Swiss National Science Foundation (SNSF), federal and
   cantonal authorities, Switzerland; and Academia Sinica and the National
   Science Council (NSC), former President of Academia Sinica Yuan-Tseh
   Lee, and former Ministers of NSC, Maw-Kuen Wu and Luo-Chuan Lee, Taiwan.
   We gratefully acknowledge the strong support from CERN, including
   Rolf-Dieter Heuer, and ESA. We are grateful for important discussions
   with Barry Barish, Jonathan Ellis, Neal Lane, Steve Olsen, Alvaro de
   Rujula, George Smoot, Steven Weinberg, and Frank Wilczek. The strong
   support of the flight control teams at JSC and MSFC has allowed AMS to
   operate optimally on the ISS for over three years. The work of J. Bazo,
   F. Nozzoli, and C. Pizzolotto was carried out at the ASI Science Data
   Center (ASDC) in the framework of ASI-INFN Agreement No. C/011/11/1. M.
   Vecchi is supported by the Centre national d'etudes spatiales, CNES.
   Work at Aachen University is supported by the Deutsches Zentrum fur
   Luft- und Raumfahrt, DLR, and computing resources from JARA-HPC under
   Project No. JARA0052. Work at METU is supported by the Turkish Atomic
   Energy Authority, TAEK. Work at IHEP is supported by the National
   Natural Science Foundation of China. Work at INFN-Sezione di Bologna,
   INFN-Sezione di Milano, INFN-Sezione di Perugia, INFN-Sezione di Pisa,
   INFN-TIFPA, and Universit'a di Trento, INFN-Sezione di Roma is supported
   by the Italian Space Agency, ASI, Contract No. ASI-INFN I/002/13/0. Both
   NCU and the Institute of Physics, Academia Sinica, are supported by the
   Ministry of Science and Technology. Work at CHEP, Kyungpook National
   University is supported by Grants No. NRF-2009-0080142 and No.
   NRF-2012-010226. We acknowledge computing resources from JARA-HPC under
   Project No. JARA0052. Institut fur Experimentelle Kernphysik is
   supported by the Deutsches Zentrum fur Luft- und Raumfahrt, DLR. Work at
   CIEMAT is also supported by SEIDI and CPAN. Work at UNAM is supported by
   Consejo Nacional de Ciencia y Tecnologia, CONACYT. Work at Ewha Womans
   University is supported by Grant No. NRF-2013-004883. This work was
   supported by the China Scholarship Council.
NR 30
TC 108
Z9 108
U1 16
U2 94
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 18
PY 2014
VL 113
IS 12
AR 121102
DI 10.1103/PhysRevLett.113.121102
PG 9
WC Physics, Multidisciplinary
SC Physics
GA AU7II
UT WOS:000345773700006
PM 25279617
ER

PT J
AU Lissauer, JJ
   Dawson, RI
   Tremaine, S
AF Lissauer, Jack J.
   Dawson, Rebekah I.
   Tremaine, Scott
TI Advances in exoplanet science from Kepler
SO NATURE
LA English
DT Review
ID TRANSIT TIMING VARIATIONS; MEAN-MOTION RESONANCES; LOW-DENSITY PLANETS;
   EARTH-SIZED PLANET; IN-SITU FORMATION; SOLAR-TYPE STARS; R-CIRCLE-PLUS;
   SUN-LIKE STAR; SUPER-EARTHS; ORBITAL ECCENTRICITIES
AB Numerous telescopes and techniques have been used to find and study extrasolar planets, but none has been more successful than NASA's Kepler space telescope. Kepler has discovered most of the known exoplanets, the smallest planets to orbit normal stars and the planets most likely to be similar to Earth. Most importantly, Kepler has provided us with our first look at the typical characteristics of planets and planetary systems for planets with sizes as small as, and orbits as large as, those of Earth.
C1 [Lissauer, Jack J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Dawson, Rebekah I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Tremaine, Scott] Inst Adv Study, Princeton, NJ 08540 USA.
RP Lissauer, JJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jack.lissauer@nasa.gov
RI Tremaine, Scott/M-4281-2015
OI Tremaine, Scott/0000-0002-0278-7180
FU Miller Institute for Basic Research in Science at the University of
   California, Berkeley
FX This research has made use of the Exoplanet Orbit Database at
   http://exoplanets.org and the Extrasolar Planets Encyclopedia at
   http://exoplanets.eu. We are grateful to the Kepler Science Team for
   their extensive efforts in producing the high-quality data set that has
   made possible the results reviewed here. We thank W. Borucki, E. Chiang,
   S. Dong, E. Lee, E. Lopez, L. Rogers, J. Rowe, A. Youdin and K. Zahnle
   for helpful discussions and comments on the manuscript. R.I.D. and S.T.
   gratefully acknowledge funding from the Miller Institute for Basic
   Research in Science at the University of California, Berkeley.
NR 128
TC 24
Z9 25
U1 10
U2 81
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 18
PY 2014
VL 513
IS 7518
BP 336
EP 344
DI 10.1038/nature13781
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AP1GD
UT WOS:000341814900046
PM 25230655
ER

PT J
AU Nelson, E
   van Dokkum, P
   Franx, M
   Brammer, G
   Momcheva, I
   Schreiber, NF
   da Cunha, E
   Tacconi, L
   Bezanson, R
   Kirkpatrick, A
   Leja, J
   Rix, HW
   Skelton, R
   van der Wel, A
   Whitaker, K
   Wuyts, S
AF Nelson, Erica
   van Dokkum, Pieter
   Franx, Marijn
   Brammer, Gabriel
   Momcheva, Ivelina
   Schreiber, Natascha Foerster
   da Cunha, Elisabete
   Tacconi, Linda
   Bezanson, Rachel
   Kirkpatrick, Allison
   Leja, Joel
   Rix, Hans-Walter
   Skelton, Rosalind
   van der Wel, Arjen
   Whitaker, Katherine
   Wuyts, Stijn
TI A massive galaxy in its core formation phase three billion years after
   the Big Bang
SO NATURE
LA English
DT Article
ID HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; EXTRAGALACTIC LEGACY
   SURVEY; COMPACT QUIESCENT GALAXIES; HIGH-REDSHIFT; SUBMILLIMETER
   GALAXIES; VELOCITY DISPERSIONS; METALLICITY RELATION; LARGE-SAMPLE; RED
   NUGGETS
AB Most massive galaxies are thought to have formed their dense stellar cores in early cosmic epochs(1-3). Previous studies have found galaxies with high gas velocity dispersions(4) or small apparent sizes(5-7), but so far no objects have been identified with both the stellar structure and the gas dynamics of a forming core. Here we report a candidate core in the process of formation 11 billion years ago, at redshift z = 2.3. This galaxy, GOODS-N-774, has a stellar mass of 100 billion solar masses, a half-light radius of 1.0 kiloparsecs and a star formation rate of 90(-20)(+45) solar masses per year. The star-forming gas has a velocity dispersion of 317 +/- 30 kilometres per second. This is similar to the stellar velocity dispersions of the putative descendants of GOODS-N-774, which are compact quiescent galaxies at z approximate to 2 (refs 8-11) and giant elliptical galaxies in the nearby Universe. Galaxies such as GOODS-N-774 seem to be rare; however, from the star formation rate and size of this galaxy weinfer that many star-forming cores may be heavily obscured, and could be missed in optical and near-infrared surveys.
C1 [Nelson, Erica; van Dokkum, Pieter; Momcheva, Ivelina; Leja, Joel] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
   [Franx, Marijn] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
   [Brammer, Gabriel] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Schreiber, Natascha Foerster; Tacconi, Linda; Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
   [da Cunha, Elisabete; Rix, Hans-Walter; van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
   [Bezanson, Rachel] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
   [Kirkpatrick, Allison] Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA.
   [Skelton, Rosalind] South African Astron Observ, ZA-7935 Cape Town, South Africa.
   [Whitaker, Katherine] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Nelson, E (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA.
EM erica.nelson@yale.edu
OI Leja, Joel/0000-0001-6755-1315; da Cunha, Elisabete/0000-0001-9759-4797
FU STScI [GO-1277]
FX Support from STScI grant GO-1277 is acknowledged.
NR 46
TC 28
Z9 28
U1 0
U2 6
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 18
PY 2014
VL 513
IS 7518
BP 394
EP +
DI 10.1038/nature13616
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AP1GD
UT WOS:000341814900054
PM 25162527
ER

PT J
AU Ott, M
   Pierson, D
   Shirakawa, M
   Tanigaki, F
   Hida, M
   Yamazaki, T
   Shimazu, T
   Ishioka, N
AF Ott, Mark
   Pierson, Duane
   Shirakawa, Masaki
   Tanigaki, Fumiaki
   Hida, Masamitsu
   Yamazaki, Takashi
   Shimazu, Toru
   Ishioka, Noriaki
CA Natl Aeronautics Space Adm
   Japan Aerosp Exploration Agcy JAXA
TI Space Habitation and Microbiology: Status and Roadmap of Space Agencies
SO MICROBES AND ENVIRONMENTS
LA English
DT Editorial Material
ID STATION; MODULE; KIBO
C1 [Ott, Mark; Pierson, Duane] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
   [Shirakawa, Masaki; Tanigaki, Fumiaki; Hida, Masamitsu; Yamazaki, Takashi] Japan Aerosp Explorat Agcy JAXA, Human Spaceflight Mission Directorate, Space Environm Utilizat Ctr, Tsukuba, Ibaraki 3058505, Japan.
   [Yamazaki, Takashi] Teikyo Univ, Grad Sch Med, Lab Space & Environm Med, Hachioji, Tokyo 1920395, Japan.
   [Shimazu, Toru] Japan Space Forum, Chiyoda Ku, Tokyo 1010062, Japan.
   [Ishioka, Noriaki] Japan Space Explorat Agcy JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
RP Ishioka, N (reprint author), Japan Space Explorat Agcy JAXA, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
EM ishioka.noriaki@jaxa.jp
NR 12
TC 2
Z9 2
U1 2
U2 10
PU JAPANESE SOC MICROBIAL ECOLOGY, DEPT BIORESOURCE SCIENCE
PI IBARAKI
PA C/O DR. HIROYUKI OHTA, SEC, IBARAKI UNIV COLLEGE OF AGRICULT, AMI-MACHI,
   IBARAKI, JAPAN
SN 1342-6311
J9 MICROBES ENVIRON
JI Microbes Environ.
PD SEP 17
PY 2014
VL 29
IS 3
BP 239
EP 242
DI 10.1264/jsme2.ME2903rh
PG 4
WC Biotechnology & Applied Microbiology; Microbiology
SC Biotechnology & Applied Microbiology; Microbiology
GA AP6XI
UT WOS:000342221400001
PM 25130884
ER

PT J
AU Venkateswaran, K
   La Duc, MT
   Horneck, G
AF Venkateswaran, Kasthuri
   La Duc, Myron T.
   Horneck, Gerda
TI Microbial Existence in Controlled Habitats and Their Resistance to Space
   Conditions
SO MICROBES AND ENVIRONMENTS
LA English
DT Review
DE Closed habitat; International Space Station; PLANET PROTECT; BOSS;
   Microbial Observatory
ID SUPEROXIDE DISMUTASE; MARTIAN ATMOSPHERE; OUTER-SPACE; CLEAN ROOMS;
   EXPOSE-E; ENVIRONMENT; SURVIVAL; MISSION; ASTROBIOLOGY; DIVERSITY
AB The National Research Council (NRC) has recently recognized the International Space Station (ISS) as uniquely suitable for furthering the study of microbial species in closed habitats. Answering the NRC's call for the study, in particular, of uncommon microbial species in the ISS, and/or of those that have significantly increased or decreased in number, space microbiologists have begun capitalizing on the maturity, speed, and cost-effectiveness of molecular/genomic microbiological technologies to elucidate changes in microbial populations in the ISS and other closed habitats. Since investigators can only collect samples infrequently from the ISS itself due to logistical reasons, Earth analogs, such as spacecraft-assembly clean rooms, are used and extensively characterized for the presence of microbes. Microbiologists identify the predominant, problematic, and extremophilic microbial species in these closed habitats and use the ISS as a testbed to study their resistance to extreme extraterrestrial environmental conditions. Investigators monitor the microbes exposed to the real space conditions in order to track their genomic changes in response to the selective pressures present in outer space (external to the ISS) and the spaceflight (in the interior of the ISS). In this review, we discussed the presence of microbes in space research-related closed habitats and the resistance of some microbial species to the extreme environmental conditions of space.
C1 [Venkateswaran, Kasthuri; La Duc, Myron T.] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA.
   [Horneck, Gerda] DLR German Aerosp Ctr, Inst Aerosp Med, D-51170 Cologne, Germany.
RP Venkateswaran, K (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA.
EM kjvenkat@jpl.nasa.gov
FU Space Biology [NNH12ZTT001N, 19-12829-26, NNN13D111T]; National
   Aeronautics and Space Administration [TP 475]
FX The research described herein was carried out in part at the Jet
   Propulsion Laboratory, California Institute of Technology, under a
   contract with the National Aeronautics and Space Administration, and in
   part (EXPOSE-experiments) at the DLR, within the DLR-FuW Program TP 475
   "ISS utilization and biodiagnostics." This research was funded by 2012
   Space Biology NNH12ZTT001N grant # 19-12829-26 under Task Order
   NNN13D111T. The authors acknowledge the JPL Biotechnology and Planetary
   Protection Group for their research conducted under NASA's Mars Program.
   The PROTECT team thanks the astronauts who were involved in the exposure
   and retrieval of EXPOSE-E samples; the team at ESA's European Space
   Research and Technology Centre during EXPOSE-E planning, operation, and
   evaluation; and the team at DLR's Microgravity User Support Center, who
   contributed to the EXPOSE-E preparation, engineering verification
   testing, and ground simulation experiments. The authors are grateful to
   Dr. Petra Rettberg for her invitation to participate in future BOSS
   flight experiments. Permission to reproduce some of the information
   given in this review article was obtained from the respective journals.
NR 54
TC 5
Z9 5
U1 7
U2 28
PU JAPANESE SOC MICROBIAL ECOLOGY, DEPT BIORESOURCE SCIENCE
PI IBARAKI
PA C/O DR. HIROYUKI OHTA, SEC, IBARAKI UNIV COLLEGE OF AGRICULT, AMI-MACHI,
   IBARAKI, JAPAN
SN 1342-6311
J9 MICROBES ENVIRON
JI Microbes Environ.
PD SEP 17
PY 2014
VL 29
IS 3
BP 243
EP 249
DI 10.1264/jsme2.ME14032
PG 7
WC Biotechnology & Applied Microbiology; Microbiology
SC Biotechnology & Applied Microbiology; Microbiology
GA AP6XI
UT WOS:000342221400002
PM 25130881
ER

PT J
AU Yamaguchi, N
   Roberts, M
   Castro, S
   Oubre, C
   Makimura, K
   Leys, N
   Grohmann, E
   Sugita, T
   Ichijo, T
   Nasu, M
AF Yamaguchi, Nobuyasu
   Roberts, Michael
   Castro, Sarah
   Oubre, Cherie
   Makimura, Koichi
   Leys, Natalie
   Grohmann, Elisabeth
   Sugita, Takashi
   Ichijo, Tomoaki
   Nasu, Masao
TI Microbial Monitoring of Crewed Habitats in Space-Current Status and
   Future Perspectives
SO MICROBES AND ENVIRONMENTS
LA English
DT Review
DE International Space Station; microbial monitoring; on-site analysis
ID SHEAR MODELED MICROGRAVITY; ESCHERICHIA-COLI; SIMULATED MICROGRAVITY;
   BIOFILM FORMATION; STAPHYLOCOCCUS-AUREUS; GENE-EXPRESSION;
   CANDIDA-ALBICANS; REDUCED GRAVITY; FLOW CYTOMETER; BACTERIAL
AB Previous space research conducted during short-term flight experiments and long-term environmental monitoring on board orbiting space stations suggests that the relationship between humans and microbes is altered in the crewed habitat in space. Both human physiology and microbial communities adapt to spaceflight. Microbial monitoring is critical to crew safety in long-duration space habitation and the sustained operation of life support systems on space transit vehicles, space stations, and surface habitats. To address this critical need, space agencies including NASA (National Aeronautics and Space Administration), ESA (European Space Agency), and JAXA (Japan Aerospace Exploration Agency) are working together to develop and implement specific measures to monitor, control, and counteract biological contamination in closed-environment systems. In this review, the current status of microbial monitoring conducted in the International Space Station (ISS) as well as the results of recent microbial spaceflight experiments have been summarized and future perspectives are discussed.
C1 [Yamaguchi, Nobuyasu; Ichijo, Tomoaki; Nasu, Masao] Osaka Univ, Grad Sch Pharmaceut Sci, Suita, Osaka 5650871, Japan.
   [Roberts, Michael] NASA, CASIS, Space Life Sci Lab, Kennedy Space Ctr, FL 32899 USA.
   [Castro, Sarah] NASA, Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX 77058 USA.
   [Oubre, Cherie] Wyle, Sci Technol & Engn Grp, Houston, TX 77058 USA.
   [Makimura, Koichi] Teikyo Univ, Grad Sch Med, Lab Space & Environm Med, Hachioji, Tokyo 1920395, Japan.
   [Leys, Natalie] Belgian Nucl Res Ctr SCK CEN, BE-2400 Mol, Belgium.
   [Grohmann, Elisabeth] Univ Med Ctr Freiburg, Div Infect Dis, D-79106 Freiburg, Germany.
   [Sugita, Takashi] Meiji Pharmaceut Univ, Dept Microbiol, Kiyose, Tokyo 2048588, Japan.
RP Nasu, M (reprint author), Osaka Univ, Grad Sch Pharmaceut Sci, 1-6 Yamadaoka, Suita, Osaka 5650871, Japan.
EM nasu@phs.osaka-u.ac.jp
NR 64
TC 8
Z9 8
U1 2
U2 23
PU JAPANESE SOC MICROBIAL ECOLOGY, DEPT BIORESOURCE SCIENCE
PI IBARAKI
PA C/O DR. HIROYUKI OHTA, SEC, IBARAKI UNIV COLLEGE OF AGRICULT, AMI-MACHI,
   IBARAKI, JAPAN
SN 1342-6311
J9 MICROBES ENVIRON
JI Microbes Environ.
PD SEP 17
PY 2014
VL 29
IS 3
BP 250
EP 260
DI 10.1264/jsme2.ME14031
PG 11
WC Biotechnology & Applied Microbiology; Microbiology
SC Biotechnology & Applied Microbiology; Microbiology
GA AP6XI
UT WOS:000342221400003
PM 25130885
ER

PT J
AU Kundu, PK
   Marks, DA
   Travis, JE
AF Kundu, Prasun K.
   Marks, David A.
   Travis, James E.
TI Statistical intercomparison of idealized rainfall measurements using a
   stochastic fractional dynamics model
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GAUGE MEASUREMENTS; RADAR; TIME; SPACE; TRMM; VALIDATION; ERROR
AB A statistical method is developed for comparing precipitation data from measurements performed by (hypothetical) perfect instruments using a recently developed stochastic model of rainfall. The stochastic dynamical equation that describes the underlying random process naturally leads to a consistent spectrum and incorporates the subtle interdependence of the length and time scales governing the statistical fluctuations of the rain rate field. The main attraction of such a model is that the complete set of second-moment statistics embodied in the space-time covariance of both the area-averaged instantaneous rain rate (represented by radar or passive microwave data near the ground) and the time-averaged point rain rate (represented by rain gauge data) can be expressed as suitable integrals over the spectrum. With the help of this framework, the model allows one to carry out a faithful intercomparison of precipitation estimates derived from radar or passive microwave remote sensing over an area with direct observations by rain gauges or disdrometers, assuming all the measuring instruments to be ideal. A standard linear regression analysis approach to the intercomparison of radar and gauge rain rate estimates is formulated in terms of the appropriate observed and model-derived quantities. We also estimate the relative sampling error as well as separate absolute sampling errors for radar and gauge measurements of rainfall from the spectral model.
C1 [Kundu, Prasun K.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
   [Kundu, Prasun K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Marks, David A.] Sci Syst & Applicat Inc, Lanham, MD USA.
   [Marks, David A.] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
   [Travis, James E.] Univ Maryland Baltimore Cty, Dept Math & Stat, Baltimore, MD 21228 USA.
RP Kundu, PK (reprint author), Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
EM prasun.k.kundu@nasa.gov
FU GPM GV group as a part of the NASA Precipitation Measurement Missions
   program; JCET Fellowship
FX The research conducted in this paper was supported by the GPM GV group
   as a part of the NASA Precipitation Measurement Missions program. One of
   us (J.E.T.) gratefully acknowledges financial support from a JCET
   Fellowship. We also thank Anindya Roy for his useful comments and
   suggestions.
NR 35
TC 1
Z9 1
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 16
PY 2014
VL 119
IS 17
DI 10.1002/2014JD021509
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AQ6IN
UT WOS:000342914200004
ER

PT J
AU Roberts, YL
   Pilewskie, P
   Feldman, DR
   Kindel, BC
   Collins, WD
AF Roberts, Y. L.
   Pilewskie, P.
   Feldman, D. R.
   Kindel, B. C.
   Collins, W. D.
TI Temporal variability of observed and simulated hyperspectral reflectance
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID EMPIRICAL ORTHOGONAL FUNCTIONS; EARTH RADIATION BUDGET; ENERGY SYSTEM
   CERES; NORTHERN-HEMISPHERE; CLIMATE-CHANGE; MODEL; SCIAMACHY; CLOUDS;
   CYCLE
AB Multivariate analysis techniques were used to quantify and compare the spectral and temporal variability of observed and simulated shortwave hyperspectral Earth reflectance. The observed reflectances were measured by the Scanning Imaging Absorption Spectrometer for Atmospheric Chartography (SCIAMACHY) instrument between 2002 and 2010. The simulated reflectances were calculated using climate Observing System Simulation Experiments (OSSEs), which used two Intergovernmental Panel on Climate Change AR4 scenarios (constant CO2 and A2 emission) to drive Moderate Resolution Atmospheric Transmission simulations. Principal component (PC) spectral shapes and time series exhibited evidence of physical variables including cloud reflectance, vegetation and desert albedo, and water vapor absorption. Comparing the temporal variability of the OSSE/simulated and SCIAMACHY-measured hyperspectral reflectance showed that their Intertropical Convergence Zone-like Southern Hemisphere (SH) tropical PC1 ocean time series had a 90. phase difference. The observed and simulated PC intersection quantified their similarity and directly compared their temporal variability. The intersection showed that despite the similar spectral variability, the temporal variability of the dominant PCs differed as in, for example, the 90 degrees phase difference between the SH tropical intersection PC1s. Principal component analysis of OSSE reflectance demonstrated that the spectral and centennial variability of the two cases differed. The A2 PC time series, unlike the constant CO2 time series, exhibited centennial secular trends. Singular spectrum analysis isolated the A2 secular trends. The A2 OSSE PC1 and PC4 secular trends matched those in aerosol optical depth and total column precipitable water, respectively. This illustrates that time series of hyperspectral reflectance may be used to identify and attribute secular climate trends with a sufficiently long measurement record and high instrument accuracy.
C1 [Roberts, Y. L.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
   [Pilewskie, P.; Kindel, B. C.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
   [Pilewskie, P.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
   [Feldman, D. R.; Collins, W. D.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94720 USA.
   [Collins, W. D.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
RP Roberts, YL (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM yolanda.l.roberts@nasa.gov
RI Collins, William/J-3147-2014; Richards, Amber/K-8203-2015; Feldman,
   Daniel/N-8703-2013
OI Collins, William/0000-0002-4463-9848; Feldman,
   Daniel/0000-0003-3365-5233
FU NASA [NNX11AE71G]; NASA HQ
FX This work was supported by NASA grant NNX11AE71G and funding from NASA
   HQ for the CLARREO Project. The authors would like to thank the European
   Space Agency (ESA) for allowing the use of the SCIAMACHY data in this
   analysis (copyright ESA: 2009). The SCIAMACHY data used in this
   manuscript can be directly obtained from ESA by first completing user
   registration and calibration and finally processing the data as
   described in this manuscript. The OSSE output is stored at UC Berkeley
   and can be obtained by contacting the authors. The authors would also
   like to thank two anonymous reviewers for their comments, which have
   contributed to the significant improvement of this manuscript.
NR 41
TC 1
Z9 1
U1 0
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 16
PY 2014
VL 119
IS 17
DI 10.1002/2014JD021566
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AQ6IN
UT WOS:000342914200011
ER

PT J
AU Aponte, JC
   Dworkin, JP
   Elsila, JE
AF Aponte, Jose C.
   Dworkin, Jason P.
   Elsila, Jamie E.
TI Assessing the origins of aliphatic amines in the Murchison meteorite
   from their compound-specific carbon isotopic ratios and enantiomeric
   composition
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID CIRCULARLY-POLARIZED LIGHT; INTERSTELLAR ICE ANALOGS; MONOCARBOXYLIC
   ACIDS; MASS-SPECTROMETRY; EXTRATERRESTRIAL NUCLEOBASES;
   ULTRAVIOLET-IRRADIATION; GAS-CHROMATOGRAPHY; ORGANIC-MATTER; ALKANOIC
   ACIDS; CHONDRITES
AB The study of meteoritic organic compounds provides a unique window into the chemical inventory of the early Solar System and prebiotic chemistry that may have been important for the origin of life on Earth. Multiple families of organic compounds have been extracted from the Murchison meteorite, which is one of the most thoroughly studied carbonaceous chondrites. The amino acids extracted from Murchison have been extensively analyzed, including measurements of non-terrestrial stable isotopic ratios and discoveries of L-enantiomeric excesses for alpha-dialkyl amino acids, notably isovaline. However, although the isotopic signatures of bulk amine-containing fractions have been measured, the isotopic ratios and enantiomeric composition of individual aliphatic amines, compounds that are structurally related to amino acids, remain unknown. Here, we report a novel method for the extraction, separation, identification and quantitation of aliphatic monoamines extracted from the Murchison meteorite. Our results show a complete suite of structural isomers, with a larger concentration of methylamine and ethylamine and decreasing amine concentrations with increasing carbon number. The carbon isotopic compositions of fourteen meteoritic aliphatic monoamines were measured, with delta C-13 values ranging from +21 parts per thousand to +129 parts per thousand, showing a decrease in C-13 with increasing carbon number, a relationship that may be consistent with the chain elongation mechanism under kinetic control previously proposed for meteoritic amino acids. We also found the enantiomeric composition of sec-butylamine, a structural analog to isovaline, was racemic within error, while the isovaline extracted from the same Murchison piece showed an L-enantiomeric excess of 9.7%; this result suggested that processes leading to enantiomeric excess in the amino acid did not affect the amine. We used these collective data to assess the primordial synthetic origins of these meteoritic aliphatic amines and their potential linkage to meteoritic amino acids. (C) 2014 Elsevier Ltd. All rights reserved.
C1 [Aponte, Jose C.] NASA, Goddard Space Flight Ctr, NASA Postdoctoral Program, Greenbelt, MD 20771 USA.
   [Aponte, Jose C.; Dworkin, Jason P.; Elsila, Jamie E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Aponte, Jose C.; Dworkin, Jason P.; Elsila, Jamie E.] Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
RP Aponte, JC (reprint author), NASA, Goddard Space Flight Ctr, NASA Postdoctoral Program, 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 NASA Postdoctoral Program at the Goddard Space Flight Center; NASA
   Astrobiology Institute; Goddard Center for Astrobiology, NASA's
   Cosmochemistry Program; Simons Foundation (SCOL) [302497]; NASA
FX The authors would like to thank H. McLain for assistance in the data
   analysis of the amino acids study, T. McCoy, L. Welzenbach, and the
   Smithsonian National Museum of Natural History-Division of Meteorites
   for providing the meteorite sample used in this study, and D.P. Glavin
   for his helpful comments during preparation of the manuscript. J.C.A.
   acknowledges 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). The authors
   acknowledge Associate Editor George Cooper and two anonymous reviewers
   for their helpful comments on the manuscript.
NR 76
TC 11
Z9 11
U1 4
U2 31
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD SEP 15
PY 2014
VL 141
BP 331
EP 345
DI 10.1016/j.gca.2014.06.035
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2SW
UT WOS:000341926100021
ER

PT J
AU Claire, MW
   Kasting, JF
   Domagal-Goldman, SD
   Stueken, EE
   Buick, R
   Meadows, VS
AF Claire, Mark W.
   Kasting, James F.
   Domagal-Goldman, Shawn D.
   Stueeken, Eva E.
   Buick, Roger
   Meadows, Victoria S.
TI Modeling the signature of sulfur mass-independent fractionation produced
   in the Archean atmosphere
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID MICROBIAL SULFATE REDUCTION; BILLION YEARS AGO; MULTIPLE-SULFUR; EARLY
   EARTH; SOUTH-AFRICA; ISOTOPE RECORDS; CARBONYL SULFIDE; GREENSTONE-BELT;
   UV PHOTOLYSIS; ORGANIC HAZE
AB Minor sulfur isotope anomalies indicate the absence of O-2 from the Archean atmosphere. A rich dataset showing large variations in magnitude and sign of Delta S-33 and Delta S-36, preserved in both sulfates and sulfides, suggests that further constraints on Archean atmospheric chemistry are possible. We review previous quantitative constraints on atmospheric Delta S-33 production, and suggest that a new approach is needed. We added sulfur species containing S-33 and S-34 to a 1-D photochemical model and describe the numerical methodology needed to ensure accurate prediction of the magnitude and sign of Delta S-33 produced by and deposited from the Archean atmosphere. This methodology can test multiple MIF-S formation mechanisms subject to a variety of proposed atmospheric compositions, yielding Delta S-33 predictions that can be compared to the rock record. We systematically test SO2 isotopologue absorption effects in SO2 photolysis (Danielache et al., 2008), one of the primary proposed mechanisms for Delta S-33 formation. We find that differential absorption through the Danielache et al. (2008) cross sections is capable of altering predicted Delta S-33 as a function of multiple atmospheric variables, including trace O-2 concentration, total sulfur flux, CO2 content, and the presence of hydrocarbons, but find a limited role for OCS and H2S. Under all realistic conditions, the Danielache et al. (2008) cross sections yield Delta S-33 predictions at odds with the geologic record, implying that additional pathways for sulfur MIF formation exist and/or the cross sections have significant errors. The methodology presented here will allow for quantitative constraints on the Archean atmosphere beyond the absence of O-2, as soon as additional experimental measurements of MIF-S producing processes become available. (C) 2014 The Authors. Published by Elsevier Ltd.
C1 [Claire, Mark W.] Univ St Andrews, Dept Earth & Environm Sci, St Andrews KY16 9AL, Fife, Scotland.
   [Claire, Mark W.; Kasting, James F.; Domagal-Goldman, Shawn D.; Stueeken, Eva E.; Buick, Roger; Meadows, Victoria S.] Univ Washington, NASA Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA.
   [Claire, Mark W.; Domagal-Goldman, Shawn D.] Blue Marble Space Inst Sci, Seattle, WA 98109 USA.
   [Kasting, James F.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
   [Domagal-Goldman, Shawn D.] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA.
   [Stueeken, Eva E.; Buick, Roger] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
   [Meadows, Victoria S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
RP Claire, MW (reprint author), Univ St Andrews, Dept Earth & Environm Sci, Irvine Bldg, St Andrews KY16 9AL, Fife, Scotland.
EM mc229@st-andrews.ac.uk
OI Buick, Roger/0000-0003-0139-1659; Domagal-Goldman,
   Shawn/0000-0003-0354-9325
FU NAI - NASA [NNH05ZDA001C]; NASA Astrobiology Institute (NAI)
FX MC would like to thank Sebastian Danielache for providing cross-section
   data, and Aubrey Zerkle and James Farquhar for helpful conversations.
   Boz Wing and Shuhei Ono are thanked for careful reviews that improved
   this manuscript. The NASA Astrobiology Institute (NAI) is acknowledged
   for funding a NASA postdoctoral program fellowship to the lead author
   and all authors acknowledge the NAI funding for the Virtual Planetary
   Laboratory, supported by NASA under cooperative agreement NNH05ZDA001C.
NR 94
TC 18
Z9 18
U1 5
U2 45
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD SEP 15
PY 2014
VL 141
BP 365
EP 380
DI 10.1016/j.gca.2014.06.032
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AP2SW
UT WOS:000341926100023
ER

PT J
AU Francis, SP
   Lam, TTY
   McKenzie, K
   Sutton, AJ
   Ward, RL
   McClelland, DE
   Shaddock, DA
AF Francis, Samuel P.
   Lam, Timothy T-Y.
   McKenzie, Kirk
   Sutton, Andrew J.
   Ward, Robert L.
   McClelland, David E.
   Shaddock, Daniel A.
TI Weak-light phase tracking with a low cycle slip rate
SO OPTICS LETTERS
LA English
DT Article
ID LOCKING; LISA; LINK
AB The Gravity Recovery and Climate Experiment Follow-On mission will use a phase-locked loop to track changes in the phase of an optical signal that has been transmitted hundreds of kilometers between two spacecraft. Beam diffraction significantly reduces the received signal power, making it difficult to track, as the phase-locked loop is more susceptible to cycle slips. The lowest reported weak-light phase locking is at 40 fW with a cycle slip rate of 1 cycle per second. By selecting a phase-locked loop bandwidth that minimized the signal variance due to shot noise and laser phase fluctuations, a 30 fW signal has been tracked with a cycle slip rate less than 0.01 cycles per second. This is tracking at a power 25% lower with a 100-fold improvement in the cycle slip rate. This capability will enable a new class of missions, opening up new opportunities for space-based interferometry. (C) 2014 Optical Society of America
C1 [Francis, Samuel P.; Lam, Timothy T-Y.; Sutton, Andrew J.; Ward, Robert L.; McClelland, David E.; Shaddock, Daniel A.] Australian Natl Univ, Ctr Gravitat Phys, Canberra, ACT 0200, Australia.
   [McKenzie, Kirk; Sutton, Andrew J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Francis, SP (reprint author), Australian Natl Univ, Ctr Gravitat Phys, Canberra, ACT 0200, Australia.
EM samuel.francis@anu.edu.au
RI McClelland, David/E-6765-2010; Shaddock, Daniel/A-7534-2011; Ward,
   Robert/I-8032-2014
OI McClelland, David/0000-0001-6210-5842; Shaddock,
   Daniel/0000-0002-6885-3494; Ward, Robert/0000-0001-5503-5241
FU Australian Research Council; National Aeronautics and Space
   Administration (NASA)
FX This work was completed with the support of the Australian Research
   Council. Part of this research was performed at the Jet Propulsion
   Laboratory, California Institute of Technology, under contract with the
   National Aeronautics and Space Administration (NASA).
NR 16
TC 2
Z9 2
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 15
PY 2014
VL 39
IS 18
BP 5251
EP 5254
DI 10.1364/OL.39.005251
PG 4
WC Optics
SC Optics
GA AP2TA
UT WOS:000341926500003
PM 26466243
ER

PT J
AU Aasi, J
   Abbott, BP
   Abbott, R
   Abbott, T
   Abernathy, MR
   Accadia, T
   Acernese, F
   Ackley, K
   Adams, C
   Adams, T
   Addesso, P
   Adhikari, RX
   Affeldt, C
   Agathos, M
   Aggarwal, N
   Aguiar, OD
   Ain, A
   Ajith, P
   Alemic, A
   Allen, B
   Allocca, A
   Amariutei, D
   Andersen, M
   Anderson, R
   Anderson, SB
   Anderson, WG
   Arai, K
   Araya, MC
   Arceneaux, C
   Areeda, J
   Aston, SM
   Astone, P
   Aufmuth, P
   Aulbert, C
   Austin, L
   Aylott, BE
   Babak, S
   Baker, PT
   Ballardin, G
   Ballmer, SW
   Barayoga, JC
   Barbet, M
   Barish, BC
   Barker, D
   Barone, F
   Barr, B
   Barsotti, L
   Barsuglia, M
   Barton, MA
   Bartos, I
   Bassiri, R
   Basti, A
   Batch, JC
   Bauchrowitz, J
   Bauer, TS
   Behnke, B
   Bejger, M
   Beker, MG
   Belczynski, C
   Bell, AS
   Bell, C
   Bergmann, G
   Bersanetti, D
   Bertolini, A
   Betzwieser, J
   Beyersdorf, PT
   Bilenko, IA
   Billingsley, G
   Birch, J
   Biscans, S
   Bitossi, M
   Bizouard, MA
   Black, E
   Blackburn, JK
   Blackburn, L
   Blair, D
   Bloemen, S
   Blom, M
   Bock, O
   Bodiya, TP
   Boer, M
   Bogaert, G
   Bogan, C
   Bond, C
   Bondu, F
   Bonelli, L
   Bonnand, R
   Bork, R
   Born, M
   Boschi, V
   Bose, S
   Bosi, L
   Bradaschia, C
   Brady, PR
   Braginsky, VB
   Branchesi, M
   Brau, JE
   Briant, T
   Bridges, DO
   Brillet, A
   Brinkmann, M
   Brisson, V
   Brooks, AF
   Brown, DA
   Brown, DD
   Brukner, F
   Buchman, S
   Bulik, T
   Bulten, HJ
   Buonanno, A
   Burman, R
   Buskulic, D
   Buy, C
   Cadonati, L
   Cagnoli, G
   Bustillo, JC
   Calloni, E
   Camp, JB
   Campsie, P
   Cannon, KC
   Canuel, B
   Cao, J
   Capano, CD
   Carbognani, F
   Carbone, L
   Caride, S
   Castiglia, A
   Caudill, S
   Cavaglia, M
   Cavalier, F
   Cavalieri, R
   Celerier, C
   Cella, G
   Cepeda, C
   Cesarini, E
   Chakraborty, R
   Chalermsongsak, T
   Chamberlin, SJ
   Chao, S
   Charlton, P
   Chassande-Mottin, E
   Chen, X
   Chen, Y
   Chincarini, A
   Chiummo, A
   Cho, HS
   Chow, J
   Christensen, N
   Chu, Q
   Chua, SSY
   Chung, S
   Ciani, G
   Clara, F
   Clark, JA
   Cleva, F
   Coccia, E
   Cohadon, PF
   Colla, A
   Collette, C
   Colombini, M
   Cominsky, L
   Constancio, M
   Conte, A
   Cook, D
   Corbitt, TR
   Cordier, M
   Cornish, N
   Corpuz, A
   Corsi, A
   Costa, CA
   Coughlin, MW
   Coughlin, S
   Coulon, JP
   Countryman, S
   Couvares, P
   Coward, DM
   Cowart, M
   Coyne, DC
   Coyne, R
   Craig, K
   Creighton, JDE
   Creighton, TD
   Crowder, SG
   Cumming, A
   Cunningham, L
   Cuoco, E
   Dahl, K
   Dal Canton, T
   Damjanic, M
   Danilishin, SL
   D'Antonio, S
   Danzmann, K
   Dattilo, V
   Daveloza, H
   Davier, M
   Davies, GS
   Daw, EJ
   Day, R
   Dayanga, T
   Debreczeni, G
   Degallaix, J
   Deleglise, S
   Del Pozzo, W
   Denker, T
   Dent, T
   Dereli, H
   Dergachev, V
   De Rosa, R
   DeRosa, RT
   DeSalvo, R
   Dhurandhar, S
   Diaz, M
   Di Fiore, L
   Di Lieto, A
   Di Palma, I
   Di Virgilio, A
   Donath, A
   Donovan, F
   Dooley, KL
   Doravari, S
   Dossa, S
   Douglas, R
   Downes, TP
   Drago, M
   Drever, RWP
   Driggers, JC
   Du, Z
   Dwyer, S
   Eberle, T
   Edo, T
   Edwards, M
   Effler, A
   Eggenstein, H
   Ehrens, P
   Eichholz, J
   Eikenberry, SS
   Endroczi, G
   Essick, R
   Etzel, T
   Evans, M
   Evans, T
   Factourovich, M
   Fafone, V
   Fairhurst, S
   Fang, Q
   Farinon, S
   Farr, B
   Farr, WM
   Favata, M
   Fehrmann, H
   Fejer, MM
   Feldbaum, D
   Feroz, F
   Ferrante, I
   Ferrini, F
   Fidecaro, F
   Finn, LS
   Fiori, I
   Fisher, RP
   Flaminio, R
   Fournier, JD
   Franco, S
   Frasca, S
   Frasconi, F
   Frede, M
   Frei, Z
   Freise, A
   Frey, R
   Fricke, TT
   Fritschel, P
   Frolov, VV
   Fulda, P
   Fyffe, M
   Gair, J
   Gammaitoni, L
   Gaonkar, S
   Garufi, F
   Gehrels, N
   Gemme, G
   Genin, E
   Gennai, A
   Ghosh, S
   Giaime, JA
   Giardina, KD
   Giazotto, A
   Gill, C
   Gleason, J
   Goetz, E
   Goetz, R
   Gondan, L
   Gonzalez, G
   Gordon, N
   Gorodetsky, ML
   Gossan, S
   Gossler, S
   Gouaty, R
   Graf, C
   Graff, PB
   Granata, M
   Grant, A
   Gras, S
   Gray, C
   Greenhalgh, RJS
   Gretarsson, AM
   Groot, P
   Grote, H
   Grover, K
   Grunewald, S
   Guidi, GM
   Guido, C
   Gushwa, K
   Gustafson, EK
   Gustafson, R
   Hammer, D
   Hammond, G
   Hanke, M
   Hanks, J
   Hanna, C
   Hanson, J
   Harms, J
   Harry, GM
   Harry, IW
   Harstad, ED
   Hart, M
   Hartman, MT
   Haster, CJ
   Haughian, K
   Heidmann, A
   Heintze, M
   Heitmann, H
   Hello, P
   Hemming, G
   Hendry, M
   Heng, IS
   Heptonstall, AW
   Heurs, M
   Hewitson, M
   Hild, S
   Hoak, D
   Hodge, KA
   Holt, K
   Hooper, S
   Hopkins, P
   Hosken, DJ
   Hough, J
   Howell, EJ
   Hu, Y
   Huerta, E
   Hughey, B
   Husa, S
   Huttner, SH
   Huynh, M
   Huynh-Dinh, T
   Ingram, DR
   Inta, R
   Isogai, T
   Ivanov, A
   Iyer, BR
   Izumi, K
   Jacobson, M
   James, E
   Jang, H
   Jaranowski, P
   Ji, Y
   Jimenez-Forteza, F
   Johnson, WW
   Jones, DI
   Jones, R
   Jonker, RJG
   Ju, L
   Haris, K
   Kalmus, P
   Kalogera, V
   Kandhasamy, S
   Kang, G
   Kanner, JB
   Karlen, J
   Kasprzack, M
   Katsavounidis, E
   Katzman, W
   Kaufer, H
   Kawabe, K
   Kawazoe, F
   Kefelian, F
   Keiser, GM
   Keitel, D
   Kelley, DB
   Kells, W
   Khalaidovski, A
   Khalili, FY
   Khazanov, EA
   Kim, C
   Kim, K
   Kim, N
   Kim, NG
   Kim, YM
   King, EJ
   King, PJ
   Kinzel, DL
   Kissel, JS
   Klimenko, S
   Kline, J
   Koehlenbeck, S
   Kokeyama, K
   Kondrashov, V
   Koranda, S
   Korth, WZ
   Kowalska, I
   Kozak, DB
   Kremin, A
   Kringel, V
   Krishnan, B
   Krolak, A
   Kuehn, G
   Kumar, A
   Kumar, P
   Kumar, R
   Kuo, L
   Kutynia, A
   Kwee, P
   Landry, M
   Lantz, B
   Larson, S
   Lasky, PD
   Lawrie, C
   Lazzarini, A
   Lazzaro, C
   Leaci, P
   Leavey, S
   Lebigot, EO
   Lee, CH
   Lee, HK
   Lee, HM
   Lee, J
   Leonardi, M
   Leong, JR
   Le Roux, A
   Leroy, N
   Letendre, N
   Levin, Y
   Levine, B
   Lewis, J
   Li, TGF
   Libbrecht, K
   Libson, A
   Lin, AC
   Littenberg, TB
   Litvine, V
   Lockerbie, NA
   Lockett, V
   Lodhia, D
   Loew, K
   Logue, J
   Lombardi, AL
   Lorenzini, M
   Loriette, V
   Lormand, M
   Losurdo, G
   Lough, J
   Lubinski, MJ
   Luck, H
   Luijten, E
   Lundgren, AP
   Lynch, R
   Ma, Y
   Macarthur, J
   Macdonald, EP
   MacDonald, T
   Machenschalk, B
   MacInnis, M
   Macleod, DM
   Magana-Sandoval, F
   Mageswaran, M
   Maglione, C
   Mailand, K
   Majorana, E
   Maksimovic, I
   Malvezzi, V
   Man, N
   Manca, GM
   Mandel, I
   Mandic, V
   Mangano, V
   Mangini, N
   Mantovani, M
   Marchesoni, F
   Marion, F
   Marka, S
   Marka, Z
   Markosyan, A
   Maros, E
   Marque, J
   Martelli, F
   Martin, IW
   Martin, RM
   Martinelli, L
   Martynov, D
   Marx, JN
   Mason, K
   Masserot, A
   Massinger, TJ
   Matichard, F
   Matone, L
   Matzner, RA
   Mavalvala, N
   Mazumder, N
   Mazzolo, G
   McCarthy, R
   McClelland, DE
   McGuire, SC
   McIntyre, G
   McIver, J
   Mclin, K
   Meacher, D
   Meadors, GD
   Mehmet, M
   Meidam, J
   Meinders, M
   Melatos, A
   Mendell, G
   Mercer, RA
   Meshkov, S
   Messenger, C
   Meyers, P
   Miao, H
   Michel, C
   Mikhailov, EE
   Milano, L
   Milde, S
   Miller, J
   Minenkov, Y
   Mingarelli, CMF
   Mishra, C
   Mitra, S
   Mitrofanov, VP
   Mitselmakher, G
   Mittleman, R
   Moe, B
   Moesta, P
   Mohan, M
   Mohapatra, SRP
   Moraru, D
   Moreno, G
   Morgado, N
   Morriss, SR
   Mossavi, K
   Mours, B
   Mow-Lowry, CM
   Mueller, CL
   Mueller, G
   Mukherjee, S
   Mullavey, A
   Munch, J
   Murphy, D
   Murray, PG
   Mytidis, A
   Nagy, MF
   Kumar, DN
   Nardecchia, I
   Naticchioni, L
   Nayak, RK
   Necula, V
   Nelemans, G
   Neri, I
   Neri, M
   Newton, G
   Nguyen, T
   Nitz, A
   Nocera, F
   Nolting, D
   Normandin, MEN
   Nuttall, LK
   Ochsner, E
   O'Dell, J
   Oelker, E
   Oh, JJ
   Oh, SH
   Ohme, F
   Oppermann, P
   O'Reilly, B
   O'Shaughnessy, R
   Osthelder, C
   Ottaway, DJ
   Ottens, RS
   Overmier, H
   Owen, BJ
   Padilla, C
   Pai, A
   Palashov, O
   Palomba, C
   Pan, H
   Pan, Y
   Pankow, C
   Paoletti, F
   Paoletti, R
   Papa, MA
   Paris, H
   Pasqualetti, A
   Passaquieti, R
   Passuello, D
   Pedraza, M
   Penn, S
   Perreca, A
   Phelps, M
   Pichot, M
   Pickenpack, M
   Piergiovanni, F
   Pierro, V
   Pinard, L
   Pinto, IM
   Pitkin, M
   Poeld, J
   Poggiani, R
   Poteomkin, A
   Powell, J
   Prasad, J
   Premachandra, S
   Prestegard, T
   Price, LR
   Prijatelj, M
   Privitera, S
   Prix, R
   Prodi, GA
   Prokhorov, L
   Puncken, O
   Punturo, M
   Puppo, P
   Qin, J
   Quetschke, V
   Quintero, E
   Quiroga, G
   Quitzow-James, R
   Raab, FJ
   Rabeling, DS
   Racz, I
   Radkins, H
   Raffai, P
   Raja, S
   Rajalakshmi, G
   Rakhmanov, M
   Ramet, C
   Ramirez, K
   Rapagnani, P
   Raymond, V
   Re, V
   Read, J
   Reed, CM
   Regimbau, T
   Reid, S
   Reitze, DH
   Rhoades, E
   Ricci, F
   Riles, K
   Robertson, NA
   Robinet, F
   Rocchi, A
   Rodruck, M
   Rolland, L
   Rollins, JG
   Romano, R
   Romanov, G
   Romie, JH
   Rosinska, D
   Rowan, S
   Rudiger, A
   Ruggi, P
   Ryan, K
   Salemi, F
   Sammut, L
   Sandberg, V
   Sanders, JR
   Sannibale, V
   Santiago-Prieto, I
   Saracco, E
   Sassolas, B
   Sathyaprakash, BS
   Saulson, PR
   Savage, R
   Scheuer, J
   Schilling, R
   Schnabel, R
   Schofield, RMS
   Schreiber, E
   Schuette, D
   Schutz, BF
   Scott, J
   Scott, SM
   Sellers, D
   Sengupta, AS
   Sentenac, D
   Sequino, V
   Sergeev, A
   Shaddock, D
   Shah, S
   Shahriar, MS
   Shaltev, M
   Shapiro, B
   Shawhan, P
   Shoemaker, DH
   Sidery, TL
   Siellez, K
   Siemens, X
   Sigg, D
   Simakov, D
   Singer, A
   Singer, L
   Singh, R
   Sintes, AM
   Slagmolen, BJJ
   Slutsky, J
   Smith, JR
   Smith, M
   Smith, RJE
   Smith-Lefebvre, ND
   Son, EJ
   Sorazu, B
   Souradeep, T
   Sperandio, L
   Staley, A
   Stebbins, J
   Steinlechner, J
   Steinlechner, S
   Stephens, BC
   Steplewski, S
   Stevenson, S
   Stone, R
   Stops, D
   Strain, KA
   Straniero, N
   Strigin, S
   Sturani, R
   Stuver, AL
   Summerscales, TZ
   Susmithan, S
   Sutton, PJ
   Swinkels, B
   Tacca, M
   Talukder, D
   Tanner, DB
   Tarabrin, SP
   Taylor, R
   Ter Braack, APM
   Thirugnanasambandam, MP
   Thomas, M
   Thomas, P
   Thorne, KA
   Thorne, KS
   Thrane, E
   Tiwari, V
   Tokmakov, KV
   Tomlinson, C
   Toncelli, A
   Tonelli, M
   Torre, O
   Torres, CV
   Torrie, CI
   Travasso, F
   Traylor, G
   Tse, M
   Ugolini, D
   Unnikrishnan, CS
   Urban, AL
   Urbanek, K
   Vahlbruch, H
   Vajente, G
   Valdes, G
   Vallisneri, M
   van den Brand, JFJ
   Van den Broeck, C
   van der Putten, S
   van der Sluys, MV
   van Heijningen, J
   van Veggel, AA
   Vass, S
   Vasuth, M
   Vaulin, R
   Vecchio, A
   Vedovato, G
   Veitch, J
   Veitch, PJ
   Venkateswara, K
   Verkindt, D
   Verma, SS
   Vetrano, F
   Vicere, A
   Vincent-Finley, R
   Vinet, JY
   Vitale, S
   Vo, T
   Vocca, H
   Vorvick, C
   Vousden, WD
   Vyachanin, SP
   Wade, A
   Wade, L
   Wade, M
   Walker, M
   Wallace, L
   Wang, M
   Wang, X
   Ward, RL
   Was, M
   Weaver, B
   Wei, LW
   Weinert, M
   Weinstein, AJ
   Weiss, R
   Welborn, T
   Wen, L
   Wessels, P
   West, M
   Westphal, T
   Wette, K
   Whelan, JT
   White, DJ
   Whiting, BF
   Wiesner, K
   Wilkinson, C
   Williams, K
   Williams, L
   Williams, R
   Williams, T
   Williamson, AR
   Willis, JL
   Willke, B
   Wimmer, M
   Winkler, W
   Wipf, CC
   Wiseman, AG
   Wittel, H
   Woan, G
   Worden, J
   Yablon, J
   Yakushin, I
   Yamamoto, H
   Yancey, CC
   Yang, H
   Yang, Z
   Yoshida, S
   Yvert, M
   Zadrozny, A
   Zanolin, M
   Zendri, JP
   Zhang, F
   Zhang, L
   Zhao, C
   Zhu, XJ
   Zucker, ME
   Zuraw, S
   Zweizig, J
AF Aasi, J.
   Abbott, B. P.
   Abbott, R.
   Abbott, T.
   Abernathy, M. R.
   Accadia, T.
   Acernese, F.
   Ackley, K.
   Adams, C.
   Adams, T.
   Addesso, P.
   Adhikari, R. X.
   Affeldt, C.
   Agathos, M.
   Aggarwal, N.
   Aguiar, O. D.
   Ain, A.
   Ajith, P.
   Alemic, A.
   Allen, B.
   Allocca, A.
   Amariutei, D.
   Andersen, M.
   Anderson, R.
   Anderson, S. B.
   Anderson, W. G.
   Arai, K.
   Araya, M. C.
   Arceneaux, C.
   Areeda, J.
   Aston, S. M.
   Astone, P.
   Aufmuth, P.
   Aulbert, C.
   Austin, L.
   Aylott, B. E.
   Babak, S.
   Baker, P. T.
   Ballardin, G.
   Ballmer, S. W.
   Barayoga, J. C.
   Barbet, M.
   Barish, B. C.
   Barker, D.
   Barone, F.
   Barr, B.
   Barsotti, L.
   Barsuglia, M.
   Barton, M. A.
   Bartos, I.
   Bassiri, R.
   Basti, A.
   Batch, J. C.
   Bauchrowitz, J.
   Bauer, Th. S.
   Behnke, B.
   Bejger, M.
   Beker, M. G.
   Belczynski, C.
   Bell, A. S.
   Bell, C.
   Bergmann, G.
   Bersanetti, D.
   Bertolini, A.
   Betzwieser, J.
   Beyersdorf, P. T.
   Bilenko, I. A.
   Billingsley, G.
   Birch, J.
   Biscans, S.
   Bitossi, M.
   Bizouard, M. A.
   Black, E.
   Blackburn, J. K.
   Blackburn, L.
   Blair, D.
   Bloemen, S.
   Blom, M.
   Bock, O.
   Bodiya, T. P.
   Boer, M.
   Bogaert, G.
   Bogan, C.
   Bond, C.
   Bondu, F.
   Bonelli, L.
   Bonnand, R.
   Bork, R.
   Born, M.
   Boschi, V.
   Bose, Sukanta
   Bosi, L.
   Bradaschia, C.
   Brady, P. R.
   Braginsky, V. B.
   Branchesi, M.
   Brau, J. E.
   Briant, T.
   Bridges, D. O.
   Brillet, A.
   Brinkmann, M.
   Brisson, V.
   Brooks, A. F.
   Brown, D. A.
   Brown, D. D.
   Bruekner, F.
   Buchman, S.
   Bulik, T.
   Bulten, H. J.
   Buonanno, A.
   Burman, R.
   Buskulic, D.
   Buy, C.
   Cadonati, L.
   Cagnoli, G.
   Bustillo, J. Calderon
   Calloni, E.
   Camp, J. B.
   Campsie, P.
   Cannon, K. C.
   Canuel, B.
   Cao, J.
   Capano, C. D.
   Carbognani, F.
   Carbone, L.
   Caride, S.
   Castiglia, A.
   Caudill, S.
   Cavaglia, M.
   Cavalier, F.
   Cavalieri, R.
   Celerier, C.
   Cella, G.
   Cepeda, C.
   Cesarini, E.
   Chakraborty, R.
   Chalermsongsak, T.
   Chamberlin, S. J.
   Chao, S.
   Charlton, P.
   Chassande-Mottin, E.
   Chen, X.
   Chen, Y.
   Chincarini, A.
   Chiummo, A.
   Cho, H. S.
   Chow, J.
   Christensen, N.
   Chu, Q.
   Chua, S. S. Y.
   Chung, S.
   Ciani, G.
   Clara, F.
   Clark, J. A.
   Cleva, F.
   Coccia, E.
   Cohadon, P. -F.
   Colla, A.
   Collette, C.
   Colombini, M.
   Cominsky, L.
   Constancio, M., Jr.
   Conte, A.
   Cook, D.
   Corbitt, T. R.
   Cordier, M.
   Cornish, N.
   Corpuz, A.
   Corsi, A.
   Costa, C. A.
   Coughlin, M. W.
   Coughlin, S.
   Coulon, J. -P.
   Countryman, S.
   Couvares, P.
   Coward, D. M.
   Cowart, M.
   Coyne, D. C.
   Coyne, R.
   Craig, K.
   Creighton, J. D. E.
   Creighton, T. D.
   Crowder, S. G.
   Cumming, A.
   Cunningham, L.
   Cuoco, E.
   Dahl, K.
   Dal Canton, T.
   Damjanic, M.
   Danilishin, S. L.
   D'Antonio, S.
   Danzmann, K.
   Dattilo, V.
   Daveloza, H.
   Davier, M.
   Davies, G. S.
   Daw, E. J.
   Day, R.
   Dayanga, T.
   Debreczeni, G.
   Degallaix, J.
   Deleglise, S.
   Del Pozzo, W.
   Denker, T.
   Dent, T.
   Dereli, H.
   Dergachev, V.
   De Rosa, R.
   DeRosa, R. T.
   DeSalvo, R.
   Dhurandhar, S.
   Diaz, M.
   Di Fiore, L.
   Di Lieto, A.
   Di Palma, I.
   Di Virgilio, A.
   Donath, A.
   Donovan, F.
   Dooley, K. L.
   Doravari, S.
   Dossa, S.
   Douglas, R.
   Downes, T. P.
   Drago, M.
   Drever, R. W. P.
   Driggers, J. C.
   Du, Z.
   Dwyer, S.
   Eberle, T.
   Edo, T.
   Edwards, M.
   Effler, A.
   Eggenstein, H.
   Ehrens, P.
   Eichholz, J.
   Eikenberry, S. S.
   Endroczi, G.
   Essick, R.
   Etzel, T.
   Evans, M.
   Evans, T.
   Factourovich, M.
   Fafone, V.
   Fairhurst, S.
   Fang, Q.
   Farinon, S.
   Farr, B.
   Farr, W. M.
   Favata, M.
   Fehrmann, H.
   Fejer, M. M.
   Feldbaum, D.
   Feroz, F.
   Ferrante, I.
   Ferrini, F.
   Fidecaro, F.
   Finn, L. S.
   Fiori, I.
   Fisher, R. P.
   Flaminio, R.
   Fournier, J. -D.
   Franco, S.
   Frasca, S.
   Frasconi, F.
   Frede, M.
   Frei, Z.
   Freise, A.
   Frey, R.
   Fricke, T. T.
   Fritschel, P.
   Frolov, V. V.
   Fulda, P.
   Fyffe, M.
   Gair, J.
   Gammaitoni, L.
   Gaonkar, S.
   Garufi, F.
   Gehrels, N.
   Gemme, G.
   Genin, E.
   Gennai, A.
   Ghosh, S.
   Giaime, J. A.
   Giardina, K. D.
   Giazotto, A.
   Gill, C.
   Gleason, J.
   Goetz, E.
   Goetz, R.
   Gondan, L.
   Gonzalez, G.
   Gordon, N.
   Gorodetsky, M. L.
   Gossan, S.
   Gossler, S.
   Gouaty, R.
   Graef, C.
   Graff, P. B.
   Granata, M.
   Grant, A.
   Gras, S.
   Gray, C.
   Greenhalgh, R. J. S.
   Gretarsson, A. M.
   Groot, P.
   Grote, H.
   Grover, K.
   Grunewald, S.
   Guidi, G. M.
   Guido, C.
   Gushwa, K.
   Gustafson, E. K.
   Gustafson, R.
   Hammer, D.
   Hammond, G.
   Hanke, M.
   Hanks, J.
   Hanna, C.
   Hanson, J.
   Harms, J.
   Harry, G. M.
   Harry, I. W.
   Harstad, E. D.
   Hart, M.
   Hartman, M. T.
   Haster, C. -J.
   Haughian, K.
   Heidmann, A.
   Heintze, M.
   Heitmann, H.
   Hello, P.
   Hemming, G.
   Hendry, M.
   Heng, I. S.
   Heptonstall, A. W.
   Heurs, M.
   Hewitson, M.
   Hild, S.
   Hoak, D.
   Hodge, K. A.
   Holt, K.
   Hooper, S.
   Hopkins, P.
   Hosken, D. J.
   Hough, J.
   Howell, E. J.
   Hu, Y.
   Huerta, E.
   Hughey, B.
   Husa, S.
   Huttner, S. H.
   Huynh, M.
   Huynh-Dinh, T.
   Ingram, D. R.
   Inta, R.
   Isogai, T.
   Ivanov, A.
   Iyer, B. R.
   Izumi, K.
   Jacobson, M.
   James, E.
   Jang, H.
   Jaranowski, P.
   Ji, Y.
   Jimenez-Forteza, F.
   Johnson, W. W.
   Jones, D. I.
   Jones, R.
   Jonker, R. J. G.
   Ju, L.
   Haris, K.
   Kalmus, P.
   Kalogera, V.
   Kandhasamy, S.
   Kang, G.
   Kanner, J. B.
   Karlen, J.
   Kasprzack, M.
   Katsavounidis, E.
   Katzman, W.
   Kaufer, H.
   Kawabe, K.
   Kawazoe, F.
   Kefelian, F.
   Keiser, G. M.
   Keitel, D.
   Kelley, D. B.
   Kells, W.
   Khalaidovski, A.
   Khalili, F. Y.
   Khazanov, E. A.
   Kim, C.
   Kim, K.
   Kim, N.
   Kim, N. G.
   Kim, Y. -M.
   King, E. J.
   King, P. J.
   Kinzel, D. L.
   Kissel, J. S.
   Klimenko, S.
   Kline, J.
   Koehlenbeck, S.
   Kokeyama, K.
   Kondrashov, V.
   Koranda, S.
   Korth, W. Z.
   Kowalska, I.
   Kozak, D. B.
   Kremin, A.
   Kringel, V.
   Krishnan, B.
   Krolak, A.
   Kuehn, G.
   Kumar, A.
   Kumar, P.
   Kumar, R.
   Kuo, L.
   Kutynia, A.
   Kwee, P.
   Landry, M.
   Lantz, B.
   Larson, S.
   Lasky, P. D.
   Lawrie, C.
   Lazzarini, A.
   Lazzaro, C.
   Leaci, P.
   Leavey, S.
   Lebigot, E. O.
   Lee, C. -H.
   Lee, H. K.
   Lee, H. M.
   Lee, J.
   Leonardi, M.
   Leong, J. R.
   Le Roux, A.
   Leroy, N.
   Letendre, N.
   Levin, Y.
   Levine, B.
   Lewis, J.
   Li, T. G. F.
   Libbrecht, K.
   Libson, A.
   Lin, A. C.
   Littenberg, T. B.
   Litvine, V.
   Lockerbie, N. A.
   Lockett, V.
   Lodhia, D.
   Loew, K.
   Logue, J.
   Lombardi, A. L.
   Lorenzini, M.
   Loriette, V.
   Lormand, M.
   Losurdo, G.
   Lough, J.
   Lubinski, M. J.
   Lueck, H.
   Luijten, E.
   Lundgren, A. P.
   Lynch, R.
   Ma, Y.
   Macarthur, J.
   Macdonald, E. P.
   MacDonald, T.
   Machenschalk, B.
   MacInnis, M.
   Macleod, D. M.
   Magana-Sandoval, F.
   Mageswaran, M.
   Maglione, C.
   Mailand, K.
   Majorana, E.
   Maksimovic, I.
   Malvezzi, V.
   Man, N.
   Manca, G. M.
   Mandel, I.
   Mandic, V.
   Mangano, V.
   Mangini, N.
   Mantovani, M.
   Marchesoni, F.
   Marion, F.
   Marka, S.
   Marka, Z.
   Markosyan, A.
   Maros, E.
   Marque, J.
   Martelli, F.
   Martin, I. W.
   Martin, R. M.
   Martinelli, L.
   Martynov, D.
   Marx, J. N.
   Mason, K.
   Masserot, A.
   Massinger, T. J.
   Matichard, F.
   Matone, L.
   Matzner, R. A.
   Mavalvala, N.
   Mazumder, N.
   Mazzolo, G.
   McCarthy, R.
   McClelland, D. E.
   McGuire, S. C.
   McIntyre, G.
   McIver, J.
   Mclin, K.
   Meacher, D.
   Meadors, G. D.
   Mehmet, M.
   Meidam, J.
   Meinders, M.
   Melatos, A.
   Mendell, G.
   Mercer, R. A.
   Meshkov, S.
   Messenger, C.
   Meyers, P.
   Miao, H.
   Michel, C.
   Mikhailov, E. E.
   Milano, L.
   Milde, S.
   Miller, J.
   Minenkov, Y.
   Mingarelli, C. M. F.
   Mishra, C.
   Mitra, S.
   Mitrofanov, V. P.
   Mitselmakher, G.
   Mittleman, R.
   Moe, B.
   Moesta, P.
   Mohan, M.
   Mohapatra, S. R. P.
   Moraru, D.
   Moreno, G.
   Morgado, N.
   Morriss, S. R.
   Mossavi, K.
   Mours, B.
   Mow-Lowry, C. M.
   Mueller, C. L.
   Mueller, G.
   Mukherjee, S.
   Mullavey, A.
   Munch, J.
   Murphy, D.
   Murray, P. G.
   Mytidis, A.
   Nagy, M. F.
   Kumar, D. Nanda
   Nardecchia, I.
   Naticchioni, L.
   Nayak, R. K.
   Necula, V.
   Nelemans, G.
   Neri, I.
   Neri, M.
   Newton, G.
   Nguyen, T.
   Nitz, A.
   Nocera, F.
   Nolting, D.
   Normandin, M. E. N.
   Nuttall, L. K.
   Ochsner, E.
   O'Dell, J.
   Oelker, E.
   Oh, J. J.
   Oh, S. H.
   Ohme, F.
   Oppermann, P.
   O'Reilly, B.
   O'Shaughnessy, R.
   Osthelder, C.
   Ottaway, D. J.
   Ottens, R. S.
   Overmier, H.
   Owen, B. J.
   Padilla, C.
   Pai, A.
   Palashov, O.
   Palomba, C.
   Pan, H.
   Pan, Y.
   Pankow, C.
   Paoletti, F.
   Paoletti, R.
   Papa, M. A.
   Paris, H.
   Pasqualetti, A.
   Passaquieti, R.
   Passuello, D.
   Pedraza, M.
   Penn, S.
   Perreca, A.
   Phelps, M.
   Pichot, M.
   Pickenpack, M.
   Piergiovanni, F.
   Pierro, V.
   Pinard, L.
   Pinto, I. M.
   Pitkin, M.
   Poeld, J.
   Poggiani, R.
   Poteomkin, A.
   Powell, J.
   Prasad, J.
   Premachandra, S.
   Prestegard, T.
   Price, L. R.
   Prijatelj, M.
   Privitera, S.
   Prix, R.
   Prodi, G. A.
   Prokhorov, L.
   Puncken, O.
   Punturo, M.
   Puppo, P.
   Qin, J.
   Quetschke, V.
   Quintero, E.
   Quiroga, G.
   Quitzow-James, R.
   Raab, F. J.
   Rabeling, D. S.
   Racz, I.
   Radkins, H.
   Raffai, P.
   Raja, S.
   Rajalakshmi, G.
   Rakhmanov, M.
   Ramet, C.
   Ramirez, K.
   Rapagnani, P.
   Raymond, V.
   Re, V.
   Read, J.
   Reed, C. M.
   Regimbau, T.
   Reid, S.
   Reitze, D. H.
   Rhoades, E.
   Ricci, F.
   Riles, K.
   Robertson, N. A.
   Robinet, F.
   Rocchi, A.
   Rodruck, M.
   Rolland, L.
   Rollins, J. G.
   Romano, R.
   Romanov, G.
   Romie, J. H.
   Rosinska, D.
   Rowan, S.
   Ruediger, A.
   Ruggi, P.
   Ryan, K.
   Salemi, F.
   Sammut, L.
   Sandberg, V.
   Sanders, J. R.
   Sannibale, V.
   Santiago-Prieto, I.
   Saracco, E.
   Sassolas, B.
   Sathyaprakash, B. S.
   Saulson, P. R.
   Savage, R.
   Scheuer, J.
   Schilling, R.
   Schnabel, R.
   Schofield, R. M. S.
   Schreiber, E.
   Schuette, D.
   Schutz, B. F.
   Scott, J.
   Scott, S. M.
   Sellers, D.
   Sengupta, A. S.
   Sentenac, D.
   Sequino, V.
   Sergeev, A.
   Shaddock, D.
   Shah, S.
   Shahriar, M. S.
   Shaltev, M.
   Shapiro, B.
   Shawhan, P.
   Shoemaker, D. H.
   Sidery, T. L.
   Siellez, K.
   Siemens, X.
   Sigg, D.
   Simakov, D.
   Singer, A.
   Singer, L.
   Singh, R.
   Sintes, A. M.
   Slagmolen, B. J. J.
   Slutsky, J.
   Smith, J. R.
   Smith, M.
   Smith, R. J. E.
   Smith-Lefebvre, N. D.
   Son, E. J.
   Sorazu, B.
   Souradeep, T.
   Sperandio, L.
   Staley, A.
   Stebbins, J.
   Steinlechner, J.
   Steinlechner, S.
   Stephens, B. C.
   Steplewski, S.
   Stevenson, S.
   Stone, R.
   Stops, D.
   Strain, K. A.
   Straniero, N.
   Strigin, S.
   Sturani, R.
   Stuver, A. L.
   Summerscales, T. Z.
   Susmithan, S.
   Sutton, P. J.
   Swinkels, B.
   Tacca, M.
   Talukder, D.
   Tanner, D. B.
   Tarabrin, S. P.
   Taylor, R.
   Ter Braack, A. P. M.
   Thirugnanasambandam, M. P.
   Thomas, M.
   Thomas, P.
   Thorne, K. A.
   Thorne, K. S.
   Thrane, E.
   Tiwari, V.
   Tokmakov, K. V.
   Tomlinson, C.
   Toncelli, A.
   Tonelli, M.
   Torre, O.
   Torres, C. V.
   Torrie, C. I.
   Travasso, F.
   Traylor, G.
   Tse, M.
   Ugolini, D.
   Unnikrishnan, C. S.
   Urban, A. L.
   Urbanek, K.
   Vahlbruch, H.
   Vajente, G.
   Valdes, G.
   Vallisneri, M.
   van den Brand, J. F. J.
   Van den Broeck, C.
   van der Putten, S.
   van der Sluys, M. V.
   van Heijningen, J.
   van Veggel, A. A.
   Vass, S.
   Vasuth, M.
   Vaulin, R.
   Vecchio, A.
   Vedovato, G.
   Veitch, J.
   Veitch, P. J.
   Venkateswara, K.
   Verkindt, D.
   Verma, S. S.
   Vetrano, F.
   Vicere, A.
   Vincent-Finley, R.
   Vinet, J. -Y.
   Vitale, S.
   Vo, T.
   Vocca, H.
   Vorvick, C.
   Vousden, W. D.
   Vyachanin, S. P.
   Wade, A.
   Wade, L.
   Wade, M.
   Walker, M.
   Wallace, L.
   Wang, M.
   Wang, X.
   Ward, R. L.
   Was, M.
   Weaver, B.
   Wei, L. -W.
   Weinert, M.
   Weinstein, A. J.
   Weiss, R.
   Welborn, T.
   Wen, L.
   Wessels, P.
   West, M.
   Westphal, T.
   Wette, K.
   Whelan, J. T.
   White, D. J.
   Whiting, B. F.
   Wiesner, K.
   Wilkinson, C.
   Williams, K.
   Williams, L.
   Williams, R.
   Williams, T.
   Williamson, A. R.
   Willis, J. L.
   Willke, B.
   Wimmer, M.
   Winkler, W.
   Wipf, C. C.
   Wiseman, A. G.
   Wittel, H.
   Woan, G.
   Worden, J.
   Yablon, J.
   Yakushin, I.
   Yamamoto, H.
   Yancey, C. C.
   Yang, H.
   Yang, Z.
   Yoshida, S.
   Yvert, M.
   Zadrozny, A.
   Zanolin, M.
   Zendri, J. -P.
   Zhang, Fan
   Zhang, L.
   Zhao, C.
   Zhu, X. J.
   Zucker, M. E.
   Zuraw, S.
   Zweizig, J.
CA LIGO Sci Collaboration
   Virgo Collaboration
TI First all-sky search for continuous gravitational waves from unknown
   sources in binary systems
SO PHYSICAL REVIEW D
LA English
DT Article
ID MAGNETICALLY CONFINED MOUNTAIN; ACCRETING NEUTRON-STARS; RADIATION;
   STABILITY; PULSAR; X-1
AB We present the first results of an all-sky search for continuous gravitational waves from unknown spinning neutron stars in binary systems using LIGO and Virgo data. Using a specially developed analysis program, the TwoSpect algorithm, the search was carried out on data from the sixth LIGO science run and the second and third Virgo science runs. The search covers a range of frequencies from 20 Hz to 520 Hz, a range of orbital periods from 2 to similar to 2,254 h and a frequency-and period-dependent range of frequency modulation depths from 0.277 to 100 mHz. This corresponds to a range of projected semimajor axes of the orbit from similar to 0.6 x 10(-3) ls to similar to 6,500 ls assuming the orbit of the binary is circular. While no plausible candidate gravitational wave events survive the pipeline, upper limits are set on the analyzed data. The most sensitive 95% confidence upper limit obtained on gravitational wave strain is 2.3 x 10(-24) at 217 Hz, assuming the source waves are circularly polarized. Although this search has been optimized for circular binary orbits, the upper limits obtained remain valid for orbital eccentricities as large as 0.9. In addition, upper limits are placed on continuous gravitational wave emission from the low-mass x-ray binary Scorpius X-1 between 20 Hz and 57.25 Hz.
C1 [Aasi, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Anderson, R.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Barayoga, J. C.; Barish, B. C.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chakraborty, R.; Chalermsongsak, T.; Chassande-Mottin, E.; Coyne, D. C.; Dergachev, V.; Drever, R. W. P.; Driggers, J. C.; Ehrens, P.; Etzel, T.; Gushwa, K.; Gustafson, E. K.; Harms, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kanner, J. B.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D. B.; Lazzarini, A.; Lewis, J.; Li, T. G. F.; Libbrecht, K.; Litvine, V.; Mageswaran, M.; Mailand, K.; Maros, E.; Martynov, D.; Marx, J. N.; McIntyre, G.; Meshkov, S.; O'Reilly, B.; Osthelder, C.; Pedraza, M.; Phelps, M.; Price, L. R.; Privitera, S.; Quintero, E.; Raymond, V.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Singer, A.; Singer, L.; Smith, R. J. E.; Smith-Lefebvre, N. D.; Taylor, R.; Thirugnanasambandam, M. P.; Thrane, E.; Torrie, C. I.; Vass, S.; Wallace, L.; Williams, R.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
   [Abbott, T.; Corbitt, T. R.; DeRosa, R. T.; Effler, A.; Giaime, J. A.; Gonzalez, G.; Johnson, W. W.; Kokeyama, K.; Macleod, D. M.; Mullavey, A.; Singh, R.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
   [Accadia, T.; Buskulic, D.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Verkindt, D.; Yvert, M.] Univ Savoie, CNRS, Lab Annecy le Vieux Phys Particules LAPP, IN2P3, F-74941 Annecy Le Vieux, France.
   [Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Garufi, F.; Milano, L.; Romano, R.] Univ Monte S Angelo, Sez Napoli, Ist Nazl Fis Nucl, I-80126 Naples, Italy.
   [Acernese, F.; Addesso, P.; Barone, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy.
   [Ackley, K.; Amariutei, D.; Barbet, M.; Ciani, G.; Eichholz, J.; Eikenberry, S. S.; Feldbaum, D.; Fulda, P.; Gleason, J.; Goetz, R.; Hartman, M. T.; Heintze, M.; Klimenko, S.; Martin, R. M.; Mitselmakher, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Kumar, D. Nanda; Necula, V.; Ottens, R. S.; Reitze, D. H.; Tanner, D. B.; Tiwari, V.; Whiting, B. F.; Williams, L.] Univ Florida, Gainesville, FL 32611 USA.
   [Adams, C.; Aston, S. M.; Betzwieser, J.; Birch, J.; Bridges, D. O.; Cowart, M.; Doravari, S.; Evans, T.; Feldbaum, D.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Guido, C.; Hanson, J.; Heintze, M.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Kinzel, D. L.; Le Roux, A.; Lormand, M.; Nolting, D.; O'Reilly, B.; Overmier, H.; Ramet, C.; Romie, J. H.; Sellers, D.; Stuver, A. L.; Thomas, M.; Thorne, K. A.; Traylor, G.; Welborn, T.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA.
   [Adams, T.; Edwards, M.; Fairhurst, S.; Hopkins, P.; Macdonald, E. P.; Ohme, F.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Williamson, A. R.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
   [Affeldt, C.; Allen, B.; Aulbert, C.; Bauchrowitz, J.; Bergmann, G.; Bock, O.; Bogan, C.; Born, M.; Brinkmann, M.; Dahl, K.; Dal Canton, T.; Damjanic, M.; Danzmann, K.; Denker, T.; Dent, T.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Eggenstein, H.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Goetz, E.; Gossler, S.; Grote, H.; Hanke, M.; Heurs, M.; Hewitson, M.; Kawazoe, F.; Keitel, D.; Khalaidovski, A.; Koehlenbeck, S.; Kringel, V.; Krishnan, B.; Kuehn, G.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Manca, G. M.; Mazzolo, G.; Mehmet, M.; Mossavi, K.; Mow-Lowry, C. M.; Oppermann, P.; Pickenpack, M.; Poeld, J.; Prix, R.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schreiber, E.; Schuette, D.; Shaltev, M.; Simakov, D.; Slutsky, J.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Was, M.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Wiesner, K.; Willke, B.; Wimmer, M.; Winkler, W.; Wittel, H.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
   [Agathos, M.; Bauer, Th. S.; Beker, M. G.; Bertolini, A.; Bloemen, S.; Blom, M.; Bulten, H. J.; Del Pozzo, W.; Ghosh, S.; Jonker, R. J. G.; Li, T. G. F.; Meidam, J.; Nelemans, G.; Rabeling, D. S.; Shah, S.; Ter Braack, A. P. M.; van den Brand, J. F. J.; Van den Broeck, C.; van der Putten, S.; van der Sluys, M. V.; van Heijningen, J.; Veitch, J.] Nikhef, NL-1098 XG Amsterdam, Netherlands.
   [Aggarwal, N.; Barsotti, L.; Biscans, S.; Bodiya, T. P.; Donovan, F.; Essick, R.; Evans, M.; Fritschel, P.; Gras, S.; Isogai, T.; Katsavounidis, E.; Kwee, P.; Lee, J.; Libson, A.; Lynch, R.; MacInnis, M.; Mason, K.; Matichard, F.; Mavalvala, N.; Miller, J.; Mittleman, R.; Oelker, E.; Shoemaker, D. H.; Tse, M.; Vaulin, R.; Vitale, S.; Weiss, R.; Wipf, C. C.; Zhang, Fan; Zucker, M. E.] MIT, LIGO, Cambridge, MA 02139 USA.
   [Aguiar, O. D.; Constancio, M., Jr.; Costa, C. A.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
   [Ain, A.; Bose, Sukanta; Dhurandhar, S.; Gaonkar, S.; Mitra, S.; Prasad, J.; Souradeep, T.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
   [Ajith, P.; Rajalakshmi, G.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
   [Alemic, A.; Ballmer, S. W.; Brown, D. A.; Couvares, P.; Fisher, R. P.; Harry, I. W.; Kelley, D. B.; Kumar, P.; Lough, J.; Magana-Sandoval, F.; Massinger, T. J.; Mohapatra, S. R. P.; Nitz, A.; Perreca, A.; Saulson, P. R.; West, M.] Syracuse Univ, New York, NY 13244 USA.
   [Allen, B.; Anderson, W. G.; Brady, P. R.; Caudill, S.; Chamberlin, S. J.; Creighton, J. D. E.; Downes, T. P.; Hammer, D.; Huynh, M.; Kline, J.; Koranda, S.; Mercer, R. A.; Moe, B.; Nuttall, L. K.; Ochsner, E.; O'Shaughnessy, R.; Pankow, C.; Papa, M. A.; Siemens, X.; Stephens, B. C.; Urban, A. L.; Wade, L.; Wade, M.; Wiseman, A. G.] Univ Wisconsin, Milwaukee, WI 53201 USA.
   [Allen, B.; Aufmuth, P.; Danzmann, K.; Kaufer, H.; Lueck, H.; Mazzolo, G.; Meinders, M.; Schnabel, R.; Vahlbruch, H.; Willke, B.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
   [Allocca, A.; Basti, A.; Bitossi, M.; Bonelli, L.; Boschi, V.; Bradaschia, C.; Cella, G.; Di Lieto, A.; Di Virgilio, A.; Ferrante, I.; Fidecaro, F.; Frasconi, F.; Gennai, A.; Giazotto, A.; Mantovani, M.; Paoletti, F.; Paoletti, R.; Passaquieti, R.; Passuello, D.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Torre, O.; Vajente, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
   [Allocca, A.; Paoletti, R.; Torre, O.] Univ Siena, I-53100 Siena, Italy.
   [Andersen, M.; Bassiri, R.; Buchman, S.; Celerier, C.; Fejer, M. M.; Keiser, G. M.; Kim, N.; Lantz, B.; Lin, A. C.; MacDonald, T.; Markosyan, A.; Shapiro, B.; Stebbins, J.; Urbanek, K.] Stanford Univ, Stanford, CA 94305 USA.
   [Arceneaux, C.; Cavaglia, M.; Kandhasamy, S.] Univ Mississippi, University, MS 38677 USA.
   [Areeda, J.; Lockett, V.; Padilla, C.; Read, J.; Smith, J. R.] Calif State Univ Fullerton, Fullerton, CA 92831 USA.
   [Astone, P.; Colla, A.; Conte, A.; Frasca, S.; Majorana, E.; Mangano, V.; Naticchioni, L.; Palomba, C.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
   [Aylott, B. E.; Bond, C.; Brown, D. D.; Bruekner, F.; Carbone, L.; Farr, W. M.; Freise, A.; Grover, K.; Haster, C. -J.; Lodhia, D.; Mandel, I.; Mingarelli, C. M. F.; Sidery, T. L.; Stevenson, S.; Stops, D.; Vecchio, A.; Vousden, W. D.; Wang, M.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
   [Babak, S.; Behnke, B.; Donath, A.; Grunewald, S.; Leaci, P.; Milde, S.; Papa, M. A.; Schutz, B. F.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
   [Baker, P. T.; Cornish, N.] Montana State Univ, Bozeman, MT 59717 USA.
   [Ballardin, G.; Canuel, B.; Carbognani, F.; Cavalieri, R.; Chiummo, A.; Cuoco, E.; Dattilo, V.; Day, R.; Ferrini, F.; Fiori, I.; Genin, E.; Hemming, G.; Kasprzack, M.; Marque, J.; Mohan, M.; Nocera, F.; Paoletti, F.; Pasqualetti, A.; Prijatelj, M.; Ruggi, P.; Sentenac, D.; Swinkels, B.] European Gravitat Observ, I-56021 Pisa, Italy.
   [Barker, D.; Barton, M. A.; Batch, J. C.; Clara, F.; Cook, D.; Dwyer, S.; Gray, C.; Hanks, J.; Ingram, D. R.; Izumi, K.; Kawabe, K.; Kissel, J. S.; Landry, M.; Levine, B.; Lubinski, M. J.; McCarthy, R.; Mendell, G.; Moraru, D.; Moreno, G.; Paris, H.; Raab, F. J.; Radkins, H.; Reed, C. M.; Rodruck, M.; Ryan, K.; Sandberg, V.; Savage, R.; Sigg, D.; Thomas, P.; Vo, T.; Vorvick, C.; Weaver, B.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA.
   [Barr, B.; Bell, A. S.; Bell, C.; Campsie, P.; Craig, K.; Cumming, A.; Cunningham, L.; Davies, G. S.; Douglas, R.; Gill, C.; Gordon, N.; Graef, C.; Grant, A.; Hammond, G.; Hart, M.; Haughian, K.; Hendry, M.; Heng, I. S.; Hild, S.; Hough, J.; Hu, Y.; Huttner, S. H.; Jones, R.; Kumar, R.; Lawrie, C.; Leavey, S.; Logue, J.; Macarthur, J.; Martin, I. W.; Messenger, C.; Murray, P. G.; Newton, G.; Pitkin, M.; Powell, J.; Robertson, N. A.; Rowan, S.; Santiago-Prieto, I.; Scott, J.; Sorazu, B.; Strain, K. A.; Torrie, C. I.; van Veggel, A. A.; Woan, G.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
   [Barsuglia, M.; Buy, C.; Chassande-Mottin, E.; Tacca, M.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, Observ Paris,Sorbonne Paris Cite,, F-75205 Paris 13, France.
   [Bartos, I.; Countryman, S.; Factourovich, M.; Marka, S.; Marka, Z.; Matone, L.; Murphy, D.; Staley, A.; Tse, M.] Columbia Univ, New York, NY 10027 USA.
   [Basti, A.; Bonelli, L.; Di Lieto, A.; Ferrante, I.; Fidecaro, F.; Passaquieti, R.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Vajente, G.] Univ Pisa, I-56127 Pisa, Italy.
   [Bejger, M.; Rosinska, D.] CAMK PAN, PL-00716 Warsaw, Poland.
   [Belczynski, C.; Bulik, T.; Kowalska, I.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
   [Bersanetti, D.; Chincarini, A.; Farinon, S.; Gemme, G.; Neri, M.; Pierro, V.; Pinto, I. M.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy.
   [Bersanetti, D.; Neri, M.] Univ Genoa, I-16146 Genoa, Italy.
   [Beyersdorf, P. T.; Cordier, M.] San Jose State Univ, San Jose, CA 95192 USA.
   [Bilenko, I. A.; Braginsky, V. B.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L.; Strigin, S.; Vyachanin, S. P.] Moscow MV Lomonosov State Univ, Fac Phys, Moscow 119991, Russia.
   [Bizouard, M. A.; Brisson, V.; Cavalier, F.; Davier, M.; Franco, S.; Hello, P.; Kasprzack, M.; Leroy, N.; Robinet, F.] Univ Paris 11, LAL, IN2P3, CNRS, F-91898 Orsay, France.
   [Blackburn, L.; Camp, J. B.; Gehrels, N.; Graff, P. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Blair, D.; Burman, R.; Chen, X.; Chu, Q.; Chung, S.; Coward, D. M.; Danilishin, S. L.; Fang, Q.; Hooper, S.; Howell, E. J.; Ju, L.; Ma, Y.; Qin, J.; Susmithan, S.; Verma, S. S.; Wen, L.; Zhao, C.; Zhu, X. J.] Univ Western Australia, Crawley, WA 6009, Australia.
   [Bloemen, S.; Ghosh, S.; Groot, P.; Nelemans, G.; Shah, S.; van der Sluys, M. V.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
   [Boer, M.; Bogaert, G.; Brillet, A.; Cleva, F.; Coulon, J. -P.; Dereli, H.; Fournier, J. -D.; Heitmann, H.; Kefelian, F.; Man, N.; Martinelli, L.; Meacher, D.; Pichot, M.; Regimbau, T.; Siellez, K.; Vinet, J. -Y.; Wei, L. -W.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice, France.
   [Bondu, F.] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France.
   [Bonnand, R.; Cagnoli, G.; Degallaix, J.; Flaminio, R.; Granata, M.; Michel, C.; Morgado, N.; Pinard, L.; Saracco, E.; Sassolas, B.; Straniero, N.] Univ Lyon, IN2P3, CNRS, Lab Mat Avances, F-69622 Lyon, France.
   [Bose, Sukanta; Dayanga, T.; Ghosh, S.; Steplewski, S.] Washington State Univ, Pullman, WA 99164 USA.
   [Bosi, L.; Colombini, M.; Gammaitoni, L.; Marchesoni, F.; Neri, I.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
   [Branchesi, M.; Guidi, G. M.; Losurdo, G.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Florence, Italy.
   [Branchesi, M.; Guidi, G. M.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Univ Urbino Carlo Bo, I-61029 Urbino, Italy.
   [Brau, J. E.; Frey, R.; Harstad, E. D.; Quitzow-James, R.; Schofield, R. M. S.; Talukder, D.] Univ Oregon, Eugene, OR 97403 USA.
   [Briant, T.; Cohadon, P. -F.; Deleglise, S.; Heidmann, A.] Univ Paris 06, CNRS, ENS, Lab Kastler Brossel, F-75005 Paris, France.
   [Bulten, H. J.; Rabeling, D. S.; van den Brand, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands.
   [Buonanno, A.; Capano, C. D.; Pan, Y.; Shawhan, P.; Yancey, C. C.] Univ Maryland, College Pk, MD 20742 USA.
   [Cadonati, L.; Clark, J. A.; Hoak, D.; Karlen, J.; Lombardi, A. L.; Mangini, N.; McIver, J.; Zuraw, S.] Univ Massachusetts, Amherst, MA 01003 USA.
   [Bustillo, J. Calderon; Husa, S.; Jimenez-Forteza, F.; Sintes, A. M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain.
   [Calloni, E.; De Rosa, R.; Garufi, F.; Milano, L.] Univ Naples Federico II, Complesso Univ Monte S Angelo, I-80126 Naples, Italy.
   [Cannon, K. C.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
   [Cao, J.; Du, Z.; Ji, Y.; Lebigot, E. O.; Wang, X.; Yang, Z.; Zhang, Fan] Tsinghua Univ, Beijing 100084, Peoples R China.
   [Caride, S.; Gustafson, R.; Meadors, G. D.; Riles, K.; Sanders, J. R.] Univ Michigan, Ann Arbor, MI 48109 USA.
   [Castiglia, A.; Mohapatra, S. R. P.; Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA.
   [Cesarini, E.; D'Antonio, S.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Minenkov, Y.; Nardecchia, I.; Re, V.; Rocchi, A.; Sequino, V.; Sperandio, L.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
   [Chao, S.; Kuo, L.; Pan, H.] Natl Tsing Hua Univ, Hsinchu 300, Taiwan.
   [Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
   [Chen, Y.; Gossan, S.; Miao, H.; Moesta, P.; Thorne, K. S.; Vallisneri, M.; Yang, H.] CALTECH, CaRT, Pasadena, CA 91125 USA.
   [Cho, H. S.; Kim, Y. -M.; Lee, C. -H.] Pusan Natl Univ, Pusan 609735, South Korea.
   [Chow, J.; Chua, S. S. Y.; McClelland, D. E.; Nguyen, T.; Scott, S. M.; Shaddock, D.; Slagmolen, B. J. J.; Wade, A.; Ward, R. L.] Australian Natl Univ, Canberra, ACT 0200, Australia.
   [Christensen, N.; Dossa, S.] Carleton Coll, Northfield, MN 55057 USA.
   [Coccia, E.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy.
   [Coccia, E.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Nardecchia, I.; Re, V.; Sequino, V.; Sperandio, L.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
   [Colla, A.; Conte, A.; Frasca, S.; Mangano, V.; Naticchioni, L.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy.
   [Collette, C.] Univ Brussels, B-1050 Brussels, Belgium.
   [Cominsky, L.; Mclin, K.] Sonoma State Univ, Rohnert Pk, CA 94928 USA.
   [Corpuz, A.; Gretarsson, A. M.; Hughey, B.; Loew, K.; Rhoades, E.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
   [Corsi, A.; Coyne, R.] George Washington Univ, Washington, DC 20052 USA.
   [Coughlin, M. W.; Feroz, F.; Gair, J.] Univ Cambridge, Cambridge CB2 1TN, England.
   [Coughlin, S.; Farr, B.; Kalogera, V.; Larson, S.; Littenberg, T. B.; Luijten, E.; Scheuer, J.; Shahriar, M. S.; Yablon, J.] Northwestern Univ, Evanston, IL 60208 USA.
   [Daveloza, H.; Diaz, M.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E. N.; Puncken, O.; Quetschke, V.; Rakhmanov, M.; Ramirez, K.; Stone, R.; Torres, C. V.; Valdes, G.] Univ Texas Brownsville, Brownsville, TX 78520 USA.
   [Kremin, A.; Mandic, V.; Meyers, P.; Prestegard, T.] Univ Minnesota, Minneapolis, MN 55455 USA.
   [Daw, E. J.; Edo, T.; Tomlinson, C.; White, D. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
   [Debreczeni, G.; Endroczi, G.; Nagy, M. F.; Racz, I.; Vasuth, M.] RMKI, Wigner RCP, H-1121 Budapest, Hungary.
   [DeSalvo, R.; Pierro, V.; Pinto, I. M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
   [Drago, M.; Leonardi, M.; Prodi, G. A.] Ist Nazl Fis Nucl, Grp Collegato Trento, I-38050 Trento, Italy.
   [Drago, M.; Leonardi, M.; Prodi, G. A.] Univ Trent, I-38050 Trento, Italy.
   [Favata, M.] Montclair State Coll, Montclair, NJ 07043 USA.
   [Finn, L. S.; Inta, R.; Owen, B. J.] Penn State Univ, University Pk, PA 16802 USA.
   [Frei, Z.; Gondan, L.; Raffai, P.] MTA Eotvos Univ, Lendulet ARG, H-1117 Budapest, Hungary.
   [Gammaitoni, L.; Neri, I.; Travasso, F.; Vocca, H.] Univ Perugia, I-06123 Perugia, Italy.
   [Greenhalgh, R. J. S.; O'Dell, J.] HSIC, Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
   [Hanna, C.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
   [Harry, G. M.] Amer Univ, Washington, DC 20016 USA.
   [Hosken, D. J.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
   [Iyer, B. R.] Raman Res Inst, Bangalore 560080, Karnataka, India.
   [Jang, H.; Kang, G.; Kim, C.; Kim, N. G.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea.
   [Jaranowski, P.] Bialystok Univ, PL-15424 Bialystok, Poland.
   [Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
   [Haris, K.; Mazumder, N.; Mishra, C.; Pai, A.] IISER TVM, Trivandrum 695016, Kerala, India.
   [Khazanov, E. A.; Palashov, O.; Poteomkin, A.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
   [Kim, C.; Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
   [Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
   [Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
   [Krolak, A.; Kutynia, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
   [Kumar, A.] Inst Plasma Res, Bhat 382428, Gandhinagar, India.
   [Lasky, P. D.; Melatos, A.; Sammut, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
   [Lazzaro, C.; Vedovato, G.; Zendri, J. -P.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
   [Levin, Y.; Premachandra, S.] Monash Univ, Clayton, Vic 3800, Australia.
   [Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
   [Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
   [Maglione, C.; Quiroga, G.] Argentinian Gravitat Wave Grp, RA-5000 Cordoba, Argentina.
   [Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy.
   [Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA.
   [McGuire, S. C.; Vincent-Finley, R.; Williams, K.] Southern Univ, Baton Rouge, LA 70813 USA.
   [McGuire, S. C.; Vincent-Finley, R.; Williams, K.] A&M Coll, Baton Rouge, LA 70813 USA.
   [Mikhailov, E. E.; Romanov, G.] Coll William & Mary, Williamsburg, VA 23187 USA.
   [Nayak, R. K.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
   [Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Taejon 305390, South Korea.
   [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
   [Raja, S.] RRCAT, Indore 452013, MP, India.
   [Reid, S.] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland.
   [Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
   [Sengupta, A. S.] Indian Inst Technol, Gandhi Sagar 382424, India.
   [Sturani, R.] Univ Estadual Paulista, Int Ctr Theoret Phys, South Amer Inst Res, Inst Fis Teor, BR-01140070 Sao Paulo, Brazil.
   [Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
   [Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
   [Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
   [Williams, T.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
   [Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
EM evan.goetz@aei.mpg.de
RI Howell, Eric/H-5072-2014; Frey, Raymond/E-2830-2016; Ciani,
   Giacomo/G-1036-2011; Di Virgilio, Angela Dora Vittoria/E-9078-2015;
   Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Ward,
   Robert/I-8032-2014; Frasconi, Franco/K-1068-2016; Groot,
   Paul/K-4391-2016; Lazzaro, Claudia/L-2986-2016; Pinto,
   Innocenzo/L-3520-2016; Ferrante, Isidoro/F-1017-2012; Losurdo,
   Giovanni/K-1241-2014; Travasso, Flavio/J-9595-2016; Bartos,
   Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella,
   Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Costa,
   Cesar/G-7588-2012; Chow, Jong/A-3183-2008; Aggarwal, Nancy/M-7203-2015;
   Shaddock, Daniel/A-7534-2011; Vicere, Andrea/J-1742-2012; Rocchi,
   Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Branchesi,
   Marica/P-2296-2015; Strain, Kenneth/D-5236-2011; Miao,
   Haixing/O-1300-2013; Gehring, Tobias/A-8596-2016; Heidmann,
   Antoine/G-4295-2016; Nelemans, Gijs/D-3177-2012; Marchesoni,
   Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; Vecchio,
   Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Strigin,
   Sergey/I-8337-2012; Leonardi, Matteo/G-9694-2015; Sigg,
   Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015;
   Graef, Christian/J-3167-2015; Bell, Angus/E-7312-2011; Ottaway,
   David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise,
   Samuel/B-1599-2015; Neri, Igor/F-1482-2010; Steinlechner,
   Sebastian/D-5781-2013; Gammaitoni, Luca/B-5375-2009; Khalili,
   Farit/D-8113-2012; Gorodetsky, Michael/C-5938-2008; McClelland,
   David/E-6765-2010; Hild, Stefan/A-3864-2010; M, Manjunath/N-4000-2014;
   Gemme, Gianluca/C-7233-2008; Iyer, Bala R./E-2894-2012; prodi,
   giovanni/B-4398-2010; Canuel, Benjamin/C-7459-2014; Danilishin,
   Stefan/K-7262-2012; Prokhorov, Leonid/I-2953-2012; 
OI O'Shaughnessy, Richard/0000-0001-5832-8517; Allen,
   Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Kanner,
   Jonah/0000-0001-8115-0577; Freise, Andreas/0000-0001-6586-9901; Denker,
   Timo/0000-0003-1259-5315; Naticchioni, Luca/0000-0003-2918-0730;
   calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515;
   Sorazu, Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735;
   Bondu, Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397;
   Del Pozzo, Walter/0000-0003-3978-2030; Pinto, Innocenzo
   M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Guidi,
   Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431;
   Collette, Christophe/0000-0002-4430-3703; Pierro,
   Vincenzo/0000-0002-6020-5521; Coccia, Eugenio/0000-0002-6669-5787;
   Vetrano, Flavio/0000-0002-7523-4296; Addesso, Paolo/0000-0003-0895-184X;
   Vedovato, Gabriele/0000-0001-7226-1320; Howell,
   Eric/0000-0001-7891-2817; Boschi, Valerio/0000-0001-8665-2293;
   Matichard, Fabrice/0000-0001-8982-8418; Husa,
   Sascha/0000-0002-0445-1971; Papa, M.Alessandra/0000-0002-1007-5298;
   Vocca, Helios/0000-0002-1200-3917; Aulbert, Carsten/0000-0002-1481-8319;
   Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338;
   Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Goetz,
   Evan/0000-0003-2666-721X; Swinkels, Bas/0000-0002-3066-3601; Ward,
   Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan,
   John/0000-0001-5710-6576; Frasconi, Franco/0000-0003-4204-6587; Groot,
   Paul/0000-0002-4488-726X; Lazzaro, Claudia/0000-0001-5993-3372;
   Ferrante, Isidoro/0000-0002-0083-7228; Losurdo,
   Giovanni/0000-0003-0452-746X; Travasso, Flavio/0000-0002-4653-6156;
   Punturo, Michele/0000-0001-8722-4485; Cella,
   Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167;
   Chow, Jong/0000-0002-2414-5402; Shaddock, Daniel/0000-0002-6885-3494;
   Vicere, Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016;
   Martelli, Filippo/0000-0003-3761-8616; Strain,
   Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958; Gehring,
   Tobias/0000-0002-4311-2593; Heidmann, Antoine/0000-0002-0784-5175;
   Nelemans, Gijs/0000-0002-0752-2974; Marchesoni,
   Fabio/0000-0001-9240-6793; Zhu, Xingjiang/0000-0001-7049-6468; Vecchio,
   Alberto/0000-0002-6254-1617; Sigg, Daniel/0000-0003-4606-6526; Puppo,
   Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef,
   Christian/0000-0002-4535-2603; Bell, Angus/0000-0003-1523-0821; Garufi,
   Fabio/0000-0003-1391-6168; Deleglise, Samuel/0000-0002-8680-5170; Neri,
   Igor/0000-0002-9047-9822; Steinlechner, Sebastian/0000-0003-4710-8548;
   Gammaitoni, Luca/0000-0002-4972-7062; Gorodetsky,
   Michael/0000-0002-5159-2742; McClelland, David/0000-0001-6210-5842; M,
   Manjunath/0000-0001-8710-0730; Gemme, Gianluca/0000-0002-1127-7406;
   Iyer, Bala R./0000-0002-4141-5179; prodi, giovanni/0000-0001-5256-915X;
   Danilishin, Stefan/0000-0001-7758-7493; Nitz,
   Alexander/0000-0002-1850-4587; Mandel, Ilya/0000-0002-6134-8946;
   Whiting, Bernard F/0000-0002-8501-8669; Veitch,
   John/0000-0002-6508-0713; Davies, Gareth/0000-0002-4289-3439; Pitkin,
   Matthew/0000-0003-4548-526X; Murphy, David/0000-0002-8538-815X
FU Australian Research Council; International Science Linkages program of
   the Commonwealth of Australia; Council of Scientific and Industrial
   Research of India; Istituto Nazionale di Fisica Nucleare of Italy;
   Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia
   Hisenda i Innovacio of the Govern de les Illes Balears; Netherlands
   Organisation for Scientific Research; Polish Ministry of Science and
   Higher Education; FOCUS Programme of Foundation for Polish Science;
   Royal Society; Scottish Funding Council; Scottish Universities Physics
   Alliance; National Aeronautics and Space Administration; OTKA of
   Hungary; Lyon Institute of Origins (LIO); National Research Foundation
   of Korea; Industry Canada and the Province of Ontario through the
   Ministry of Economic Development and Innovation; National Science and
   Engineering Research Council Canada; Carnegie Trust; Leverhulme Trust;
   David and Lucile Packard Foundation; Research Corporation; Alfred P.
   Sloan Foundation; LIGO [LIGO-P1300048]
FX The authors gratefully acknowledge the support of the United States
   National Science Foundation for the construction and operation of the
   LIGO Laboratory; the Science and Technology Facilities Council of the
   United Kingdom, the Max-Planck-Society, and the State of
   Niedersachsen/Germany for support of the construction and operation of
   the GEO600 detector; and the Italian Istituto Nazionale di Fisica
   Nucleare and the French Centre National de la Recherche Scientifique for
   the construction and operation of the Virgo detector. The authors also
   gratefully acknowledge the support of the research by these agencies and
   by the Australian Research Council, the International Science Linkages
   program of the Commonwealth of Australia, the Council of Scientific and
   Industrial Research of India, the Istituto Nazionale di Fisica Nucleare
   of Italy, the Spanish Ministerio de Economia y Competitividad, the
   Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes
   Balears, the Foundation for Fundamental Research on Matter supported by
   the Netherlands Organisation for Scientific Research, the Polish
   Ministry of Science and Higher Education, the FOCUS Programme of
   Foundation for Polish Science, the Royal Society, the Scottish Funding
   Council, the Scottish Universities Physics Alliance, the National
   Aeronautics and Space Administration, OTKA of Hungary, the Lyon
   Institute of Origins (LIO), the National Research Foundation of Korea,
   Industry Canada and the Province of Ontario through the Ministry of
   Economic Development and Innovation, the National Science and
   Engineering Research Council Canada, the Carnegie Trust, the Leverhulme
   Trust, the David and Lucile Packard Foundation, the Research
   Corporation, and the Alfred P. Sloan Foundation. This article has LIGO
   Document No. LIGO-P1300048.
NR 44
TC 22
Z9 22
U1 3
U2 50
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 15
PY 2014
VL 90
IS 6
DI 10.1103/PhysRevD.90.062010
PG 17
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AP5TR
UT WOS:000342142100001
ER

PT J
AU Badavi, FF
AF Badavi, Francis F.
TI Validation of the new trapped environment AE9/AP9/SPM at low Earth orbit
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Radiation belts; Anisotropy; Space station; Low Earth orbit
ID SPACE-STATION; MODEL; ANISOTROPY; FLUX; ISS; PROTONS
AB The completion of the international space station (ISS) in 2011 has provided the space research community an ideal proving ground for future long duration human activities in space. Ionizing radiation measurements in ISS form the ideal tool for the validation of radiation environmental models, nuclear transport codes and nuclear reaction cross sections. Indeed, prior measurements on the space transportation system (STS; shuttle) provided vital information impacting both the environmental models and the nuclear transport code developments by indicating the need for an improved dynamic model of the low Earth orbit (LEO) trapped environment. Additional studies using thermo-luminescent detector (TLD), tissue equivalent proportional counter (TEPC) area monitors, and computer aided design (CAD) model of earlier ISS configurations, confirmed STS observations that, as input, computational dosimetry requires an environmental model with dynamic and directional (anisotropic) behavior, as well as an accurate six degree of freedom (DOF) definition of the vehicle attitude and orientation along the orbit of ISS.
   At LEO, a vehicle encounters exposure from trapped particles and attenuated galactic cosmic rays (GCR). Within the trapped field, a challenge arises from properly estimating the amount of exposure acquired. There exist a number of models to define the intensities of the trapped particles during the solar quiet and active times. At active times, solar energetic particles (SEP) generated by solar flare or coronal mass ejection (CME) also contribute to the exposure at high northern and southern latitudes. Among the more established trapped models are the historic and popular AE8/AP8, dating back to the 1980s, the historic and less popular CRRES electron/proton, dating back to 1990s and the recently released AE9/AP9/SPM. The AE9/AP9/SPM model is a major improvement over the older AE8/AP8 and CRRES models. This model is derived from numerous measurements acquired over four solar cycles dating back to the 1970s, roughly representing 40 years of data collection. In contrast, the older AE8/AP8 and CRRES models were limited to only a few months of measurements taken during the prior solar minima and maxima.
   The dual goal of this paper is to first validate the AE8/AP8 and AE9/AP9/SPM trapped models against ISS dosemetric measurements for a silicon based detector, to assess the improvements in the AE9/AP9/SPM model as compared to AE8/AP8 model. The validation is done at selected target points within ISS-6A configuration during its passage through the south Atlantic anomaly (SAA). For such validation, only the isotropic spectrum of either model is needed.
   As a second goal, the isotropic spectra of both trapped models are re-casted into anisotropic spectra by modulating them with a measurement derived angular formalism which is applicable to trapped protons. Since at LEO electrons have minimal exposure contribution, the paper ignores the AE8 and AE9 component of the models and presents the angular validation of AP8 and AP9 against measurements from the compact environment anomaly sensor (CEASE) science instrument package, flown onboard the tri-service experiment-5 (TSX-5) satellite during the period of June 2000-July 2006. The spin stabilized satellite. was flown in a 410 x 1710 km, 69 degrees inclination orbit, allowing it to be exposed to a broad range of LEO regime. Particular emphasize is put on the validation of proton flux profiles at differential 40 MeV and integral >40 MeV, in the vicinity of SAA where protons exhibit east-west (EW) anisotropy and have a relatively narrow pitch angle distribution. Within SAA, the EW anisotropy results in different level of exposure to each side of CEASE instrument package, allowing the extraction of anisotropic proton spectra from the measurements. While the magnitude of the EW effect at LEO depends on a multitude of factors such as trapped proton energy, orientation of the spacecraft along the velocity vector and altitude of the spacecraft, for this part, the paper draws quantitative conclusions on the combined effect of proton pitch angle and EW anomaly. (C) 2014 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Badavi, Francis F.] Old Dominion Univ, Norfolk, VA 23529 USA.
RP Badavi, FF (reprint author), NASA, Langley Res Ctr, MS 188E, Hampton, VA 23681 USA.
EM francis.f.badavi@nasa.gov
FU NASA [NNX12AN58A]
FX The author wishes to express his gratitude to G.P. Ginet of MIT Lincoln
   Laboratory for providing information on the TSX-5 CEASE detector, to
   W.R. Johnston of Space Vehicles Directorate, Air Force Research
   Laboratory, Kirtland AFB and T.P. O'Brien of Aerospace Corporation for
   assistance with the AE9/AP9/SPM trapped model. This work was partially
   supported by the NASA Grant NNX12AN58A.
NR 27
TC 2
Z9 2
U1 2
U2 10
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 2014
VL 54
IS 6
BP 917
EP 928
DI 10.1016/j.asr.2014.05.010
PG 12
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
   Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA AO4VU
UT WOS:000341340300003
ER

PT J
AU Russell, MB
   Woodall, CW
   D'Amato, AW
   Domke, GM
   Saatchi, SS
AF Russell, Matthew B.
   Woodall, Christopher W.
   D'Amato, Anthony W.
   Domke, Grant M.
   Saatchi, Sassan S.
TI Beyond mean functional traits: Influence of functional trait profiles on
   forest structure, production, and mortality across the eastern US
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE Shade tolerance; Drought tolerance; Flood tolerance; Wood density;
   Biomass; Volume
ID WESTERN UNITED-STATES; CARBON STORAGE; CLIMATE; MANAGEMENT; DIVERSITY;
   BIOMASS; STAND; BIODIVERSITY; DIFFERENCE; TOLERANCE
AB Plant functional traits (PFTs) have increased in popularity in recent years to describe various ecosystems and biological phenomena while advancing general ecological principles. To date, few have investigated distributional attributes of individual PFTs and their relationship with key attributes and processes of forest ecosystems. The objective of this study was to quantify the distribution-and contribution of various PFTs in determining forest structure, live tree production (volume and biomass), and tree mortality across the eastern US. In total, 16 metrics representing species specific gravity and their shade, flood, and drought tolerance were used to develop a PFT profile for over 23,000 permanent sample plots in the region. Spatial relationships were observed when analyzing not only the mean value of these traits but also measures of PFT complexity: the standard deviation, Shannon's index (a measure of PFT diversity), and Gini coefficient (a measure of PFT inequality). Results from nonparametric random forests models indicated that variables which formed the PFT profile contributed to explaining broad-scale patterns in the variability in forest structure (volume and biomass of overstory live trees, maximum stand density index, and tree seedling abundance; R-2 ranged from 0.09 to 0.78), production (volume [R-2 = 0.16] and biomass accretion [R-2 = 0.11]), and to a lesser degree, tree mortality. Despite the variability in the data employed and the variety of forest management regimes in these stands, this work demonstrates the utility of applying PFT profiles for understanding and predicting patterns of forest structure and production and their role in critical ecosystem processes such as carbon sequestration. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Russell, Matthew B.; D'Amato, Anthony W.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA.
   [Woodall, Christopher W.; Domke, Grant M.] USDA Forest Serv, No Res Stn, St Paul, MN 55108 USA.
   [Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Russell, MB (reprint author), Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA.
EM russellm@umn.edu
OI Domke, Grant/0000-0003-0485-0355
FU USDA Forest Service, Northern Research Station; Department of
   Interior-Northeast Climate Science Center
FX This work was supported by the USDA Forest Service, Northern Research
   Station and the Department of Interior-Northeast Climate Science Center.
   We thank David Bell, Miranda Curzon, John Stanovick and two anonymous
   reviewers for their comments that improved the content of this work and
   Brian Walters for data compilation efforts.
NR 47
TC 6
Z9 6
U1 4
U2 29
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
EI 1872-7042
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD SEP 15
PY 2014
VL 328
BP 1
EP 9
DI 10.1016/j.foreco.2014.05.014
PG 9
WC Forestry
SC Forestry
GA AO4VS
UT WOS:000341340100001
ER

PT J
AU Jaumann, R
   Nass, A
   Otto, K
   Krohn, K
   Stephan, K
   McCord, TB
   Williams, DA
   Raymond, CA
   Blewett, DT
   Hiesinger, H
   Yingst, RA
   De Sanctis, MC
   Palomba, E
   Roatsch, T
   Matz, KD
   Preusker, F
   Scholten, F
   Russell, CT
AF Jaumann, R.
   Nass, A.
   Otto, K.
   Krohn, K.
   Stephan, K.
   McCord, T. B.
   Williams, D. A.
   Raymond, C. A.
   Blewett, D. T.
   Hiesinger, H.
   Yingst, R. A.
   De Sanctis, M. C.
   Palomba, E.
   Roatsch, T.
   Matz, K. -D.
   Preusker, F.
   Scholten, F.
   Russell, C. T.
TI The geological nature of dark material on Vesta and implications for the
   subsurface structure
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Geological processes; Cratering
ID ASTEROID 4 VESTA; DAWN FRAMING CAMERA; SPACE-TELESCOPE IMAGES;
   PHYSICAL-PROPERTIES; MARS-EXPRESS; SURFACE; MINERALOGY; ERUPTIONS;
   REGOLITH; CRATERS
AB Deposits of dark material appear on Vesta's surface as features of relatively low-albedo in the visible wavelength range of Dawn's camera and spectrometer. Mixed with the regolith and partially excavated by younger impacts, the material is exposed as individual layered outcrops in crater walls or ejecta patches, having been uncovered and broken up by the impact. Dark fans on crater walls and dark deposits on crater floors are the result of gravity-driven mass wasting triggered by steep slopes and impact seismicity. The fact that dark material is mixed with impact ejecta indicates that it has been processed together with the ejected material. Some small craters display continuous dark ejecta similar to lunar dark-halo impact craters, indicating that the impact excavated the material from beneath a higher-albedo surface. The asymmetric distribution of dark material in impact craters and ejecta suggests non-continuous distribution in the local subsurface. Some positive-relief dark edifices appear to be impact-sculpted hills with dark material distributed over the hill slopes. Dark features inside and outside of craters are in some places arranged as linear outcrops along scarps or as dark streaks perpendicular to the local topography. The spectral characteristics of the dark material resemble that of Vesta's regolith. Dark material is distributed unevenly across Vesta's surface with clusters of all types of dark material exposures. On a local scale, some craters expose or are associated with dark material, while others in the immediate vicinity do not show evidence for dark material. While the variety of surface exposures of dark material and their different geological correlations with surface features, as well as their uneven distribution, indicate a globally inhomogeneous distribution in the subsurface, the dark material seems to be correlated with the rim and ejecta of the older Veneneia south polar basin structure. The origin of the dark material is still being debated, however, the geological analysis suggests that it is exogenic, from carbon-rich low-velocity impactors, rather than endogenic, from freshly exposed mafic material or melt, exposed or created by impacts. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Jaumann, R.; Nass, A.; Otto, K.; Krohn, K.; Stephan, K.; Roatsch, T.; Matz, K. -D.; Preusker, F.; Scholten, F.] DLR, Inst Planetary Res, Berlin, Germany.
   [Jaumann, R.] Free Univ Berlin, Inst Geosci, Berlin, Germany.
   [McCord, T. B.] Bear Fight Inst, Winthrop, WA 98862 USA.
   [Williams, D. A.] Arizona State Univ, Tempe, AZ 85287 USA.
   [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Blewett, D. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
   [Hiesinger, H.] Univ Munster, Inst Planetol, Munster, Germany.
   [Yingst, R. A.] Planetary Sci Inst, Tucson, AZ 85719 USA.
   [De Sanctis, M. C.; Palomba, E.] INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy.
   [Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90096 USA.
RP Jaumann, R (reprint author), DLR, Inst Planetary Res, Berlin, Germany.
EM ralf.jaumann@dlr.de
RI Blewett, David/I-4904-2012; 
OI Palomba, Ernesto/0000-0002-9101-6774; Blewett,
   David/0000-0002-9241-6358; De Sanctis, Maria
   Cristina/0000-0002-3463-4437
FU DLR; Max Planck Society; NASA/JPL; AeroDynamic Solutions; Italian Space
   Agency; NASA's Dawn at Vesta Participating Scientist program, DLR;
   German Space Agency; ASI
FX The success of the Dawn mission is due to the efforts of a large team of
   engineers, scientists, and administrators in industry and government
   laboratories both in the United States and abroad. The Dawn mission is
   managed by NASA's Jet Propulsion Laboratory, a division of the
   California Institute of Technology in Pasadena, for NASA's Science
   Mission Directorate, Washington, DC. UCLA is responsible for overall
   Dawn mission science. The Dawn Framing Cameras have been developed and
   built under the leadership of the Max Planck Institute for Solar System
   Research, Katlenburg-Lindau, Germany, with significant contributions by
   DLR German Aerospace Center; Institute of Planetary Research, Berlin;
   and in coordination with the Institute of Computer and Communication
   Network Engineering, Braunschweig. The framing camera project is funded
   by DLR, the Max Planck Society, and NASA/JPL. VIR has been developed
   under the leadership of INAF-Istituto di Astrofisica e Planetologia
   Spaziali, Rome, Italy and is funded by AeroDynamic Solutions, the
   Italian Space Agency. Several of the co-authors are supported by NASA's
   Dawn at Vesta Participating Scientist program, DLR, the German Space
   Agency and ASI, the Italian Space Agency. We thank the Dawn team for the
   development, cruise, Dawn orbital insertion, and operations of the Dawn
   spacecraft at Vesta. We thank Elke Kersten and Tanja Giebner for
   supporting the preparation of maps and sketches. We also like to thank
   Matt Balme and an anonymous reviewer for their constructive comments.
   Dawn data are archived with the NASA Planetary Data System. The data
   used in this paper are available from the website
   http://dawndata.igpp.ucla.edu.
NR 59
TC 16
Z9 16
U1 2
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 15
PY 2014
VL 240
SI SI
BP 3
EP 19
DI 10.1016/j.icarus.2014.04.035
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2QY
UT WOS:000341171500002
ER

PT J
AU Longobardo, A
   Palomba, E
   Capaccioni, F
   De Sanctis, MC
   Tosi, F
   Arnmannito, E
   Schroder, SE
   Zambon, F
   Raymond, CA
   Russell, CT
AF Longobardo, Andrea
   Palomba, Ernesto
   Capaccioni, Fabrizio
   De Sanctis, Maria Cristina
   Tosi, Federico
   Arnmannito, Eleonora
   Schroeder, Stefan E.
   Zambon, Francesca
   Raymond, Carol A.
   Russell, Christopher T.
TI Photometric behavior of spectral parameters in Vesta dark and bright
   regions as inferred by the Dawn VIR spectrometer
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids, surfaces; Photometry; Spectroscopy
ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; ASTEROID 4 VESTA; RESOLVED
   PHOTOMETRY; GALILEO PHOTOMETRY; HED METEORITES; SURFACE; MISSION;
   REGOLITH; ITOKAWA; OLIVINE
AB NASA's Dawn spacecraft orbited Vesta for approximately one year, collecting thousands of hyperspectral images of its surface. The mission revealed that Vesta's surface shows the largest variations in surface albedo on asteroids visited thus far, due to the presence of dark and bright materials at the local scale (i.e. 0.1-10 km).
   The aim of this work is to characterize the photometric properties of bright and dark regions, and thus derive and apply an empirical photometric correction to all the hyperspectral observations of Vesta.
   The very large dataset (i.e. more than 20 million spectra) provided by the VIR imaging spectrometer onboard Dawn enabled accurate statistical analysis of the spectral dataset, aimed at retrieving empirical relations between several spectral parameters (i.e. visible and infrared reflectance, band depths, band centers, Band Area Ratio) and the illumination/viewing angles. The derived relations made it possible to derive photometrically corrected maps of these spectral parameters and to infer information on the regolith shadowing effect in the Vestan dark and bright regions. As an additional analysis, we also evaluated the correlation between surface temperature and band center position.
   A general conclusion of this analysis is that, from a photometric point of view, the distinction between bright and dark material units lies mainly in the larger contribution due to multiple scattering in the bright units. We observed reflectance and band depth variations over Vesta's entire surface, but these variations were much larger in the dark regions than in the bright ones.
   Band centers have been found to shift to longer wavelengths at increasing temperatures, with a trend that is the same observed for HED meteorites (Reddy et al. [2012]. Icarus 217, 153-158). Finally, the Band Area Ratio (i.e. the ratio between areas of the main pyroxene absorption bands located at 1.9 mu m and at 0.9 mu m, respectively) did not show any dependence on observational geometry, again a behavior similar to laboratory results obtained on HED meteorites (Reddy et al. [2012]. Icarus 217, 153-158). (C) 2014 Elsevier Inc. All rights reserved.
C1 [Longobardo, Andrea; Palomba, Ernesto; Capaccioni, Fabrizio; De Sanctis, Maria Cristina; Tosi, Federico; Arnmannito, Eleonora; Zambon, Francesca] INAF Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy.
   [Schroeder, Stefan E.] Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany.
   [Raymond, Carol A.] CALTECH, JPL, Pasadena, CA 91125 USA.
   [Russell, Christopher T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
RP Longobardo, A (reprint author), INAF Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere, I-00133 Rome, Italy.
EM andrea.longobardo@iaps.inaf.it
RI Schroder, Stefan/D-9709-2013; 
OI Schroder, Stefan/0000-0003-0323-8324; De Sanctis, Maria
   Cristina/0000-0002-3463-4437; Capaccioni, Fabrizio/0000-0003-1631-4314;
   Palomba, Ernesto/0000-0002-9101-6774; Tosi,
   Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592
FU Italian Space Agency-ASI; ASI; NASA
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. This work was supported by ASI and NASA.
NR 57
TC 23
Z9 23
U1 0
U2 3
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 15
PY 2014
VL 240
SI SI
BP 20
EP 35
DI 10.1016/j.icarus.2014.02.014
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2QY
UT WOS:000341171500003
ER

PT J
AU Tosi, F
   Capria, MT
   De Sanctis, MC
   Combe, JP
   Zambon, F
   Nathues, A
   Schroder, SE
   Li, JY
   Palomba, E
   Longobardo, A
   Blewett, DT
   Denevi, BW
   Palmer, E
   Capaccioni, F
   Ammannito, E
   Titus, TM
   Mittlefehldt, DW
   Sunshine, JM
   Russell, CT
   Raymond, CA
AF Tosi, F.
   Capria, M. T.
   De Sanctis, M. C.
   Combe, J. -Ph
   Zambon, F.
   Nathues, A.
   Schroeder, S. E.
   Li, J. -Y.
   Palomba, E.
   Longobardo, A.
   Blewett, D. T.
   Denevi, B. W.
   Palmer, E.
   Capaccioni, F.
   Ammannito, E.
   Titus, T. M.
   Mittlefehldt, D. W.
   Sunshine, J. M.
   Russell, C. T.
   Raymond, C. A.
CA Dawn VIR Team
TI Thermal measurements of dark and bright surface features on Vesta as
   derived from Dawn/VIR
SO ICARUS
LA English
DT Article
DE Asteroids, surfaces; Asteroid Vesta; Spectrophotometry; Infrared
   observations
ID ASTEROID 4 VESTA; HUBBLE-SPACE-TELESCOPE; FRAMING CAMERA; 21 LUTETIA;
   IMAGES; REGOLITH; SUBMILLIMETER; HETEROGENEITY; SPECTRA; SHAPE
AB Remote sensing data acquired during Dawn's orbital mission at Vesta showed several local concentrations of high-albedo (bright) and low-albedo (dark) material units, in addition to spectrally distinct meteorite impact ejecta. The thermal behavior of such areas seen at local scale (1-10 km) is related to physical properties that can provide information about the origin of those materials. We use Dawn's Visible and Infra-Red (VIR) mapping spectrometer hyperspectral data to retrieve surface temperatures and emissivities, with high accuracy as long as temperatures are greater than 220 K. Some of the dark and bright features were observed multiple times by VIR in the various mission phases at variable spatial resolution, illumination and observation angles, local solar time, and heliocentric distance. This work presents the first temperature maps and spectral emissivities of several kilometer-scale dark and bright material units on Vesta. Results retrieved from the infrared data acquired by VIR show that bright regions generally correspond to regions with lower temperature, while dark regions correspond to areas with higher temperature. During maximum daily insolation and in the range of heliocentric distances explored by Dawn, i.e. 2.23-2.54 AU, the warmest dark unit found on Vesta rises to a temperature of 273 K, while bright units observed under comparable conditions do not exceed 266 K. Similarly, dark units appear to have higher emissivity on average compared to bright units. Dark-material units show a weak anticorrelation between temperature and albedo, whereas the relation is stronger for bright material units observed under the same conditions. Individual features may show either evanescent or distinct margins in the thermal images, as a consequence of the cohesion of the surface material. Finally, for the two categories of dark and bright materials, we were able to highlight the influence of heliocentric distance on surface temperatures, and estimate an average temperature rate change of 1% following a variation of 0.04 AU in the solar distance. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Tosi, F.; Capria, M. T.; De Sanctis, M. C.; Zambon, F.; Palomba, E.; Longobardo, A.; Capaccioni, F.; Ammannito, E.] INAF IAPS Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy.
   [Combe, J. -Ph] Bear Fight Inst, Winthrop, WA 98862 USA.
   [Nathues, A.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
   [Schroeder, S. E.] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany.
   [Li, J. -Y.; Palmer, E.] Planetary Sci Inst, Tucson, AZ 85719 USA.
   [Blewett, D. T.; Denevi, B. W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
   [Titus, T. M.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
   [Mittlefehldt, D. W.] NASA Johnson Space Ctr, Houston, TX 77058 USA.
   [Sunshine, J. M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 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 Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
EM federico.tosi@iaps.inaf.it
RI Blewett, David/I-4904-2012; Schroder, Stefan/D-9709-2013; Denevi,
   Brett/I-6502-2012; 
OI Capaccioni, Fabrizio/0000-0003-1631-4314; Palomba,
   Ernesto/0000-0002-9101-6774; Tosi, Federico/0000-0003-4002-2434; Zambon,
   Francesca/0000-0002-4190-6592; Blewett, David/0000-0002-9241-6358;
   Schroder, Stefan/0000-0003-0323-8324; Denevi, Brett/0000-0001-7837-6663;
   capria, maria teresa/0000-0002-9814-9588; De Sanctis, Maria
   Cristina/0000-0002-3463-4437
FU Italian Space Agency (ASI), ASI-INAF [I/004/12/0]; NASA Dawn at Vesta
   Participating Scientist program
FX This work was supported by the Italian Space Agency (ASI), ASI-INAF
   Contract I/004/12/0. The authors would like to thank the Dawn Science,
   Operation and Instrument Teams for a successful Dawn at Vesta mission.
   Several of the authors 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 Sharon Uy for her assistance in revising the manuscript, and two
   anonymous reviewers for their useful comments. We warmly thank Robert
   Gaskell (PSI) for providing a detailed shape model of Vesta that was
   used in this work. Dawn datasets are publicly available at the Planetary
   Data System Small Bodies Node (http://pdssbn.astro.umd.edu/). The
   computational resources used in this research have been supplied by
   INAF-IAPS through the DataWell project.
NR 57
TC 29
Z9 29
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 15
PY 2014
VL 240
SI SI
BP 36
EP 57
DI 10.1016/j.icarus.2014.03.017
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2QY
UT WOS:000341171500004
ER

PT J
AU Palomba, E
   Longobardo, A
   De Sanctis, MC
   Zambon, F
   Tosi, F
   Ammannito, E
   Capaccioni, F
   Frigeri, A
   Capria, MT
   Cloutis, EA
   Jaumann, R
   Combe, JP
   Raymond, CA
   Russell, CT
AF Palomba, Ernesto
   Longobardo, Andrea
   De Sanctis, Maria Cristina
   Zambon, Francesca
   Tosi, Federico
   Ammannito, Eleonora
   Capaccioni, Fabrizio
   Frigeri, Alessandro
   Capria, Maria Teresa
   Cloutis, Edward A.
   Jaumann, Ralf
   Combe, Jean-Philippe
   Raymond, Carol A.
   Russell, Christopher T.
TI Composition and mineralogy of dark material units on Vesta
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Spectroscopy; Asteroids, surfaces; Mineralogy; Regoliths
ID ASTEROID 4 VESTA; ORGANIC-MATTER; HED METEORITES; DAWN MISSION; 21
   LUTETIA; SURFACE; REGOLITH; SPECTRA; HETEROGENEITY; TEMPERATURE
AB Vesta is the asteroid with the largest albedo variation among the known rocky Solar System objects and shows a widespread occurrence of dark material (DM) and bright material (BM) units. In the first observation phases by the Dawn spacecraft, two main extensions of low albedo areas were identified on Vesta and found to be closely correlated with carbonaceous, OH-rich, material. In this work we use the hyper-spectral data provided by the VIR-Dawn imaging spectrometer onboard Dawn to detect and analyze individual, well-defined, dark material units. We define DM units assuming a relative criterion, i.e. reflectance lower than the surroundings. By coupling visible and infrared images of the same area we are able to select real dark material units, discarding false detections created by shadowing effects. A detailed final catalogue of 123 dark units is presented, containing the geographical parameters and the main spectral characteristics for each unit. Independently of the geological context of the dark units, all DMs show similar spectral properties, dominated by the pyroxene absorption features, as is the average spectrum of Vesta. This finding suggests a similar composition, with the presence of darkening agents that also weaken pyroxene band depths. The majority (90%) of the DM units shows a positive correlation between low albedo and an OH band centered at 2.8 mu m, confirming the hypothesis that the darkening agents are carbonaceous chondrites, probably delivered by low-velocity impacts of primitive asteroids. A comparison with laboratory spectra allows us to better constrain the size and the composition of the darkening agents. These DM areas seem to be made of eucritic material. The regolith grain size seems to be nearly constant around an average value of 25 mu m, and is quite homogenous at least in the first hundreds of meters beneath the Vesta surface, suggesting similar processing mechanisms for both DM and BM. (C) 2014 Published by Elsevier Inc.
C1 [Palomba, Ernesto; Longobardo, Andrea; De Sanctis, Maria Cristina; Zambon, Francesca; Tosi, Federico; Ammannito, Eleonora; Capaccioni, Fabrizio; Frigeri, Alessandro; Capria, Maria Teresa] Ist Astrofis & Planetol Spaziali, INAF, I-00133 Rome, Italy.
   [Ammannito, Eleonora; Russell, Christopher T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
   [Cloutis, Edward A.] Univ Winnipeg, Winnipeg, MB R3B 2E9, Canada.
   [Jaumann, Ralf] DLR, Berlin, Germany.
   [Combe, Jean-Philippe] Bear Fight Inst, Winthrop, WA 98862 USA.
   [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Palomba, E (reprint author), Ist Astrofis & Planetol Spaziali, INAF, Via Fosso Cavaliere, I-00133 Rome, Italy.
EM ernesto.palomba@iaps.inaf.it
RI Frigeri, Alessandro/F-2151-2010; 
OI Frigeri, Alessandro/0000-0002-9140-3977; capria, maria
   teresa/0000-0002-9814-9588; De Sanctis, Maria
   Cristina/0000-0002-3463-4437; Capaccioni, Fabrizio/0000-0003-1631-4314;
   Palomba, Ernesto/0000-0002-9101-6774; Tosi,
   Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592
FU Italian Space Agency-ASI; ASI-Italy; NASA-United States
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. This work was supported by ASI-Italy and NASA-United
   States. A portion of this work was performed at the NASALIPL. We warmly
   thank Sharon Uy (UCLA) for manuscript revisions, Vishnu Reddy (PSI) for
   ample discussions about spectral parameters, S. Marchi for fruitful
   discussions about the DM origin scenarios, Paul C. Buchanan, Tasha Dunn
   and an anonymous reviewer for thorough and very constructive reviews
   which helped to improve our manuscript. The data used in this paper are
   available from the website http://dawndata.igpp.ucla.edu.
NR 70
TC 19
Z9 19
U1 3
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 SEP 15
PY 2014
VL 240
SI SI
BP 58
EP 72
DI 10.1016/j.icarus.2014.04.040
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2QY
UT WOS:000341171500005
ER

PT J
AU Zambon, F
   Sanctis, MCB
   Schroder, S
   Tosi, F
   Longobardo, A
   Ammannito, E
   Blewett, DT
   Mittlefehldt, DW
   Li, JY
   Palomba, E
   Capaccioni, F
   Frigeri, A
   Capria, MT
   Fonte, S
   Nathues, A
   Pieters, CM
   Russell, CT
   Raymond, CA
AF Zambon, F.
   Sanctis, Maria Cristina Be
   Schroeder, Stefan
   Tosi, Federico
   Longobardo, Andrea
   Ammannito, Eleonora
   Blewett, David T.
   Mittlefehldt, David W.
   Li, Jian-Yang
   Palomba, E.
   Capaccioni, Fabrizio
   Frigeri, Alessandro
   Capria, Maria Teresa
   Fonte, Sergio
   Nathues, Andreas
   Pieters, Carle M.
   Russell, Christofer T.
   Raymond, Carol A.
TI Spectral analysis of the bright materials on the asteroid Vesta
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Spectroscopy; Mineralogy
ID REFLECTANCE SPECTRA; PYROXENE MIXTURES; MINERAL MIXTURES;
   INFRARED-SPECTRA; DARK MATERIAL; DAWN MISSION; GRAIN-SIZE; LUNAR SOIL;
   OLIVINE; SURFACE
AB Vesta spectra have prominent near-infrared absorption bands characteristic of pyroxenes, indicating a direct link to the howardite, eucrite and diogenite meteorites. Many localized dark and bright materials are present on Vesta's surface. Here we focus on the bright material (BM) units to determine their spectral properties, their origin, the presence of mineralogical phases different from pyroxenes, and whether different bright units share a common lithology. VIR, the Visible and Infrared spectrometer onboard Dawn, allows us to first do a detailed analysis of the spectral properties of a large number of bright material units on Vesta including examples of the different morphological classes. The spectral parameters used are band centers, band depths, and Band Area Ratio (BAR) for the pyroxene bands at similar to 0.9 and similar to 1.9 mu m. The mineralogies of most bright regions are consistent with those of the howardite, eucrite and diogenite meteorites typical of Vesta's surface. We find that bright material units exhibit the full range of HED pyroxene composition, from eucrites to diogenites. Large part of the bright materials are eucrite-rich, according with the Vesta's mineralogy. In most cases, the bright materials have the same mineralogy of the surrounding terrain, but have larger band depth values. The band depths can be related to the abundance of the absorbing minerals, the abundance of Fe2+, grain size, and/or to the abundance of opaque materials. We found a positive correlation between albedo and band depth, which suggests that the grain size is not the main factor responsible for the higher albedo. The analysis of the band parameters indicates that most of the bright materials, excluding the few olivine-rich units, represent fresh uncontaminated Vestan pyroxenes from a variety of lithologies exposed from beneath the surface by impacts. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Zambon, F.; Sanctis, Maria Cristina Be; Tosi, Federico; Longobardo, Andrea; Ammannito, Eleonora; Palomba, E.; Capaccioni, Fabrizio; Frigeri, Alessandro; Capria, Maria Teresa; Fonte, Sergio] INAF IAPS Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy.
   [Schroeder, Stefan] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany.
   [Blewett, David T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
   [Mittlefehldt, David W.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
   [Li, Jian-Yang] Planetary Sci Inst, Tucson, AZ 85719 USA.
   [Nathues, Andreas] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
   [Pieters, Carle M.] Brown Univ, Providence, RI 02912 USA.
   [Russell, Christofer T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
   [Raymond, Carol A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Raymond, Carol A.] CALTECH, Pasadena, CA 91109 USA.
RP Zambon, F (reprint author), INAF IAPS Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
EM francesca.zambon@iaps.inaf.it
RI Blewett, David/I-4904-2012; Schroder, Stefan/D-9709-2013; Frigeri,
   Alessandro/F-2151-2010; 
OI Blewett, David/0000-0002-9241-6358; capria, maria
   teresa/0000-0002-9814-9588; De Sanctis, Maria
   Cristina/0000-0002-3463-4437; Capaccioni, Fabrizio/0000-0003-1631-4314;
   Palomba, Ernesto/0000-0002-9101-6774; Tosi,
   Federico/0000-0003-4002-2434; Schroder, Stefan/0000-0003-0323-8324;
   Frigeri, Alessandro/0000-0002-9140-3977; Zambon,
   Francesca/0000-0002-4190-6592
FU Italian Space Agency (ASI); NASA's Dawn at Vesta Participating
   Scientists Program
FX This work was supported by the Italian Space Agency (ASI) and NASA's
   Dawn at Vesta Participating Scientists 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. The authors acknowledge the Dawn Science, Operation and
   Instrument Teams. A special acknowledgment to Dr. Cristian Carli for his
   helpful comments.
NR 75
TC 18
Z9 18
U1 2
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 2014
VL 240
SI SI
BP 73
EP 85
DI 10.1016/j.icarus.2014.04.037
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2QY
UT WOS:000341171500006
ER

PT J
AU Konopliv, AS
   Asmar, SW
   Park, RS
   Bills, BG
   Centinello, F
   Chamberlin, AB
   Ermakov, A
   Gaskell, RW
   Rambaux, N
   Raymond, CA
   Russell, CT
   Smith, DE
   Tricarico, P
   Zuber, MT
AF Konopliv, A. S.
   Asmar, S. W.
   Park, R. S.
   Bills, B. G.
   Centinello, F.
   Chamberlin, A. B.
   Ermakov, A.
   Gaskell, R. W.
   Rambaux, N.
   Raymond, C. A.
   Russell, C. T.
   Smith, D. E.
   Tricarico, P.
   Zuber, M. T.
TI The Vesta gravity field, spin pole and rotation period, landmark
   positions, and ephemeris from the Dawn tracking and optical data
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids, dynamics; Asteroids, rotation; Geophysics
ID DOPPLER TRACKING; ASTEROID MASSES; GLOBAL SOLUTION; SPACECRAFT; IMAGES;
   ORIGIN; CERES; SHAPE; SIZE; EROS
AB The Vesta gravity field and related physical parameters have been precisely measured using 10-months of radiometric Doppler and range data and optical landmark tracking from the Dawn spacecraft. The gravity field, orientation parameters, landmark locations, and Vesta's orbit are jointly estimated. The resulting spherical harmonic gravity field has a half-wavelength resolution of 42 km (degree 20). The gravitational mass uncertainty is nearly 1 part in 10(6). The inertial spin pole location is determined to better than 0.0001 degrees and the uncertainty in the rotation period has been reduced by nearly a factor of 100. The combined precession and nutation of the pole of Vesta has been detected with angular rates about 70% of expected values, but not well enough to constrain the moment of inertia. The optical landmark position estimates reduce the uncertainty in the center-of-mass and center-of-figure offset to 10 m. The Vesta ephemeris uncertainty during the Dawn stay was reduced from 20 km to better than 10 m in the Earth-Vesta direction. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Konopliv, A. S.; Asmar, S. W.; Park, R. S.; Bills, B. G.; Chamberlin, A. B.; Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Centinello, F.; Ermakov, A.; Zuber, M. T.] MIT, Cambridge, MA 02139 USA.
   [Gaskell, R. W.; Tricarico, P.] Planetary Sci Inst, Tucson, AZ 85719 USA.
   [Rambaux, N.] Univ Paris 06, Paris, France.
   [Rambaux, N.] Observ Paris, CNRS, UMR 8028, IMCCE, F-75014 Paris, France.
   [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
   [Smith, D. E.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
RP Konopliv, AS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM alex.konopliv@jpl.nasa.gov
OI Ermakov, Anton/0000-0002-7020-7061
NR 53
TC 22
Z9 22
U1 0
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 SEP 15
PY 2014
VL 240
SI SI
BP 103
EP 117
DI 10.1016/j.icarus.2013.09.005
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2QY
UT WOS:000341171500008
ER

PT J
AU Park, RS
   Konopliv, AS
   Asmar, SW
   Bills, BG
   Gaskell, RW
   Raymond, CA
   Smith, DE
   Toplis, MJ
   Zuber, MT
AF Park, R. S.
   Konopliv, A. S.
   Asmar, S. W.
   Bills, B. G.
   Gaskell, R. W.
   Raymond, C. A.
   Smith, D. E.
   Toplis, M. J.
   Zuber, M. T.
TI Gravity field expansion in ellipsoidal harmonic and polyhedral internal
   representations applied to Vesta
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids; Asteroids, composition; Interiors; Geophysics
ID CORE FORMATION; MAGMA OCEAN; DAWN; SHAPE; DIOGENITES; EUCRITES; DENSITY;
   ORIGIN; CERES
AB A 20th degree ellipsoidal harmonic gravity field of Vesta is determined by processing radiometric Doppler and range data from the Dawn mission. The gravity field shows sensitivity up to degree 18 and the coefficients are globally determined on average to degree 15. Gravity anomalies are mapped to the Brillouin ellipsoid (304 x 289 x 247-km), which is a substantially closer fit to the surface than the reference ellipsoid (290 x 290 x 265-km) used to map the conventional spherical harmonic series, especially near the poles. Two models of internal structure are subsequently explored, in which density variations are permitted in the uppermost layer (i.e., crust) in order to explain Vesta's local gravitational signature. These models include the case of a two-layer model with an average crustal thickness of 55.5 km and a three-layer model with an average crustal thickness of 22.4 km. For both two-layer and three-layer scenarios, the Bouguer gravity anomaly is minimized for a crustal density of 2970 kg/m(3). The remaining Bouguer anomalies can be explained by lateral crustal density variation of 2310-3440 kg/m(3) and 26603240 kg/m(3) for the 22.4 km and 55.5 km crustal thickness models, respectively. The general trend of the estimated lateral crustal densities for the two cases is very similar, with a wider range for the 22.4 km case due to a thinner crust. This indicates that a thick crust (e.g., 55.5 km) would be more favorable for minimizing the range of lateral crustal density variations. Consideration of independent geochemical and petrological constraints suggests that a three-layer model is a more appropriate representation of Vesta's internal structure, despite the fact that two-layer models provide a satisfactory fit to gravity data alone. In detail, it is found that densities derived from gravity data assuming three-layer models and those derived from the howardite-eucrite-diogenite meteorites and estimates of plausible bulk-Vesta composition show an excellent level of mutual consistency. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Park, R. S.; Konopliv, A. S.; Asmar, S. W.; Bills, B. G.; Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Gaskell, R. W.] Planetaty Sci Inst, Tucson, AZ 85719 USA.
   [Smith, D. E.; Zuber, M. T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
   [Toplis, M. J.] Univ Toulouse, Observ Midi Pyrenees, CNRS, UMR 5277,Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
RP Park, RS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Ryan.S.Park@jpl.nasa.gov
NR 34
TC 15
Z9 15
U1 0
U2 9
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 15
PY 2014
VL 240
SI SI
BP 118
EP 132
DI 10.1016/j.icarus.2013.12.005
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2QY
UT WOS:000341171500009
ER

PT J
AU Ermakov, AI
   Zuber, MT
   Smith, DE
   Raymond, CA
   Balmino, G
   Fu, RR
   Ivanov, BA
AF Ermakov, Anton I.
   Zuber, Maria T.
   Smith, David E.
   Raymond, Carol A.
   Balmino, Georges
   Fu, Roger R.
   Ivanov, Boris A.
TI Constraints on Vesta's interior structure using gravity and shape models
   from the Dawn mission
SO ICARUS
LA English
DT Article
DE Asteroids, composition; Vesta; Interiors; Geophysics; Meteorites
ID ASTEROID 4 VESTA; INTERNAL STRUCTURE; UPPER-MANTLE; LUNAR CRUST; MAGMA
   OCEAN; PARENT BODY; DIOGENITES; ORIGIN; IMAGES; FIELD
AB We use the shape and gravity field of Vesta determined from observations of the Dawn spacecraft to place constraints on the asteroid's interior structure. We compute a three-layer interior structure model by minimizing the power of the residual gravity anomaly. The densities of the mantle and crust are based on constraints derived from the Howardite-Eucrite-Diogenite (HED) meteorites.
   Vesta's present-day shape is not in hydrostatic equilibrium. The Rheasilvia and Veneneia impact basins have a large effect on Vesta's shape and are the main source of deviation from hydrostatic shape. Constraining a pre-giant-impact rotation rate and orientation of the spin axis from an ellipsoidal fit to the parts of Vesta unaffected by the giant impacts, and using the theory of figure, we can constrain the shape of the core.
   Our solution for Vesta's crust-mantle interface reveals a belt of thick crust around Rheasilvia and Veneneia. The thinnest crust is in the floor of the two basins and in the Vestalia Terra region. Our solution does not reveal an uplift of the crust-mantle boundary to the surface in the largest basins. This, together with the lack of olivine detected by the Visible and Infrared Spectrometer (VIR) data in Rheasilvia and Veneneia, indicates that Vesta's presumed olivine mantle was either not brought to the surface by these large impacts or was covered by ejecta from subsequent impacts. (C) 2014 Elsevier Inc. All rights reserved.
C1 [Ermakov, Anton I.; Zuber, Maria T.; Smith, David E.; Fu, Roger R.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
   [Smith, David E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Balmino, Georges] CNES, Toulouse, France.
   [Ivanov, Boris A.] Russian Acad Sci, Inst Dynam Geospheres, Moscow, Russia.
RP Ermakov, AI (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
EM eai@mit.edu
RI Ivanov, Boris/E-1413-2016; 
OI Ivanov, Boris/0000-0002-9938-9428; Ermakov, Anton/0000-0002-7020-7061
NR 86
TC 19
Z9 19
U1 0
U2 16
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD SEP 15
PY 2014
VL 240
SI SI
BP 146
EP 160
DI 10.1016/j.icarus.2014.05.015
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2QY
UT WOS:000341171500011
ER

PT J
AU Bills, BG
   Asmar, SW
   Konopliv, AS
   Park, RS
   Raymond, CA
AF Bills, Bruce G.
   Asmar, Sami W.
   Konopliv, Alexander S.
   Park, Ryan S.
   Raymond, Carol A.
TI Harmonic and statistical analyses of the gravity and topography of Vesta
SO ICARUS
LA English
DT Article
DE Asteroid; Gravity; Topography
ID ASTEROID 4 VESTA; INTERNAL STRUCTURE; LUNAR ASYMMETRY; DAWN; MARS;
   EVOLUTION; SPHERE; IMPACT; MODEL; VENUS
AB We examine the gravity and topography of the asteroid 4 Vesta, as recently revealed by the Dawn mission. The observed gravity is highly correlated with the observed topography, and suggests little lateral variation in density. The variance spectra of both gravity and topography follow power laws which are very similar to those seen for the Moon, Mars, Venus, and Earth. A significant way in which Vesta differs from these larger silicate bodies is that both gravity and topography are significantly anisotropic, with more north-south variation than east-west variation. Rapid rotation plausibly contributes to this anisotropy, but only at harmonic degree two. The remainder of the anisotropy appears related to the large impacts which formed the Rheasilvia and Veneneia basins. We note that, as usual, gravitational inverse problems are non-unique. While the observed gravity and topography of Vesta do not preclude existence of a metallic core, they certainly do not require it. (C) 2014 Published by Elsevier Inc.
C1 [Bills, Bruce G.; Asmar, Sami W.; Konopliv, Alexander S.; Park, Ryan S.; Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bills, BG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Bruce.Bills@jpl.nasa.gov
NR 75
TC 5
Z9 5
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 SEP 15
PY 2014
VL 240
SI SI
BP 161
EP 173
DI 10.1016/j.icarus.2014.05.033
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2QY
UT WOS:000341171500012
ER

PT J
AU Coleman, M
   Meier-Augenstein, W
AF Coleman, Max
   Meier-Augenstein, Wolfram
TI Ignoring IUPAC guidelines for measurement and reporting of stable
   isotope abundance values affects us all
SO RAPID COMMUNICATIONS IN MASS SPECTROMETRY
LA English
DT Letter
ID RATIO MASS-SPECTROMETRY; COMPARATIVE EQUILIBRATION; HUMAN-HAIR;
   HYDROGEN; DELTA-O-18; SIGNATURES; ORIGIN; CARBON; FOOD
C1 [Coleman, Max] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
   [Meier-Augenstein, Wolfram] James Hutton Inst, Dundee DD2 5DA, Scotland.
RP Meier-Augenstein, W (reprint author), James Hutton Inst, Dundee DD2 5DA, Scotland.
EM wolfram.meier-augenstein@hutton.ac.uk
OI Meier-Augenstein, Wolfram/0000-0002-9498-5837
NR 22
TC 8
Z9 8
U1 3
U2 34
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0951-4198
EI 1097-0231
J9 RAPID COMMUN MASS SP
JI Rapid Commun. Mass Spectrom.
PD SEP 15
PY 2014
VL 28
IS 17
BP 1953
EP 1955
DI 10.1002/rcm.6971
PG 3
WC Biochemical Research Methods; Chemistry, Analytical; Spectroscopy
SC Biochemistry & Molecular Biology; Chemistry; Spectroscopy
GA AN2YN
UT WOS:000340452100012
PM 25088139
ER

PT J
AU Ushikubo, T
   Williford, KH
   Farquhar, J
   Johnston, DT
   Van Kranendonk, MJ
   Valley, JW
AF Ushikubo, Takayuki
   Williford, Kenneth H.
   Farquhar, James
   Johnston, David T.
   Van Kranendonk, Martin J.
   Valley, John W.
TI Development of in situ sulfur four-isotope analysis with multiple
   Faraday cup detectors by SIMS and application to pyrite grains in a
   Paleoproterozoic glaciogenic sandstone
SO CHEMICAL GEOLOGY
LA English
DT Article
DE Ion microprobe; SIMS; Sulfur isotope; S-MIF; Pyrite
ID MASS-INDEPENDENT FRACTIONATION; THERMOCHEMICAL SULFATE REDUCTION;
   ATMOSPHERIC OXYGEN; WESTERN-AUSTRALIA; ISOTOPE RECORDS; MICROPROBE
   ANALYSIS; HAMERSLEY BASIN; GREENSTONE-BELT; ION MICROPROBE; UV
   PHOTOLYSIS
AB An in situ sulfur four-isotope analysis technique with multiple Faraday cup detectors by ion microprobe was developed and applied to detrital pyrite grains in similar to 2.4 Ga glaciogenic sandstone from the Meteorite Bore Member of the Turee Creek Group, Western Australia. Data are standardized with the UWPy-1 pyrite standard (delta S-34 = 16.04 +/- 0.18 parts per thousand, Delta S-33 = -0.003 +/- 0.009 parts per thousand, and Delta S-36 = -0.21 +/- 0.24 parts per thousand, 2 SD) whose sulfur four isotopes were newly determined by gas-source mass spectrometry. Typical reproducibility at two standard deviations (2 SD) of spot-to-spot analyses of standard UWPy-1 pyrite with a primary beam size of similar to 20 mu m were +/- 0.23, +/- 0.05, and +/- 0.86 parts per thousand for delta S-34, Delta S-33, and Delta S-36, respectively. The measured S-36/S-32 ratio [1/(6641 +/- 27)] is approximately 19 parts per thousand lower than the published ratio for VCDT, and we propose a revision of the S-36 abundance in VCDT.
   Pyrite grains in similar to 2.4 Ga glaciogenic sandstone have wide ranging sulfur isotope ratios (-32.7 to 13.5 for delta S-34, -3.03 to 11.66 for Delta S-33, and -9.7 to 4.6 for Delta S-36, respectively). Some pyrite grains are zoned in delta S-34 values within a grain. Sulfur isotope ratios of most pyrite grains are distributed along a line with slope = -0.9 for Delta S-33 vs. Delta S-36, suggesting that pyrite grains mostly derived from a limited range of source rocks and near-surface sulfur reservoirs. One pyrite aggregate has a distinct texture from other pyrite grains in the same sandstone, and yields a significant mass-independent deficit in S-36 with a small excess in S-33 (Delta S-36/Delta S-33 similar to -4 parts per thousand). This is used to suggest that this grain authigenically formed by biological activity during or after sedimentation. This work demonstrates that the use of multiple Faraday cup detectors provides improved accuracy and precision for in situ sulfur four-isotope analysis with secondary ion mass spectrometry. (C) 2014 Elsevier B. V. All rights reserved.
C1 [Ushikubo, Takayuki; Williford, Kenneth H.; Valley, John W.] Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53706 USA.
   [Williford, Kenneth H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Farquhar, James] Univ Maryland, Dept Geol, College Pk, MD 20742 USA.
   [Farquhar, James] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
   [Johnston, David T.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
   [Van Kranendonk, Martin J.] Univ New S Wales, Sch Biol Earth & Environm Sci, Kensington, NSW 2052, Australia.
RP Ushikubo, T (reprint author), Japan Agcy Marine Earth Sci & Technol JAMSTEC, Kochi Inst Core Sample Res, 200 Monobe Otsu, Nankoku, Kochi 7838502, Japan.
EM ushikubot@jamstec.go.jp
OI Van Kranendonk, Martin/0000-0002-0611-2703
FU NASA Astrobiology Institute; NASA; Geological Survey of Western
   Australia;  [NSF-EAR-1053466]
FX Funding was provided by NASA Astrobiology Institute. The WiscSIMS
   laboratory is partially supported by NSF-EAR-1053466. KHW is supported
   at the Jet Propulsion Laboratory, California Institute of Technology by
   NASA. Sample collection was supported by the Geological Survey of
   Western Australia. The NSF/IF is thanked for supporting the analyses at
   Harvard University.
NR 66
TC 6
Z9 6
U1 2
U2 37
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 15
PY 2014
VL 383
BP 86
EP 99
DI 10.1016/j.chemgeo.2014.06.006
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AM9NV
UT WOS:000340209200007
ER

PT J
AU Mattioda, AL
   Bauschlicher, CW
   Bregman, JD
   Hudgins, DM
   Allamandola, LJ
   Ricca, A
AF Mattioda, Andrew L.
   Bauschlicher, Charles W., Jr.
   Bregman, Jonathan D.
   Hudgins, Douglas M.
   Allamandola, Louis J.
   Ricca, Alessandra
TI Infrared vibrational and electronic transitions in the dibenzopolyacene
   family
SO SPECTROCHIMICA ACTA PART A-MOLECULAR AND BIOMOLECULAR SPECTROSCOPY
LA English
DT Article
DE Matrix isolation; DFT; Infrared spectroscopy; Vibrational spectroscopy;
   Electronic transitions; Polycyclic aromatic hydrocarbons
ID POLYCYCLIC AROMATIC-HYDROCARBONS; EMISSION FEATURES; CORRELATION-ENERGY;
   SYMMETRY-BREAKING; PAH EMISSION; MU-M; SPECTROSCOPY; DENSITY; SPECTRA;
   HEPTACENE
AB We report experimental spectra in the mid-infrared (IR) and near-IR for a series of dibenzoacenes isolated in Ar matrices. The experiments are supported by Density Functional Theory (DFT) and Time-Dependent DFT (TD-DFT) calculations with both vibrational and electronic transitions studied. For the neutrals, we find good agreement between the experimental and B3LYP and BP86 results for all species studied. The band at about 1440 cm(-1) carries more intensity than in typical PANs and increases in intensity with the size of the dibenzoacene molecule. For the ions the B3LYP approach fails to yield reasonable IR spectra for most systems and the BP86 approach is used. Electronic transitions dominate the vibrational bands in the mid-IR region for the large dibenzoacene ions. In spite of the very strong electronic transitions, there is still reasonable agreement between theory and experiment for the vibrational band positions. The experimental and theoretical results for the dibenzoacenes are also compared with those for the polyacenes. Published by Elsevier B.V.
C1 [Mattioda, Andrew L.; Bauschlicher, Charles W., Jr.; Bregman, Jonathan D.; Hudgins, Douglas M.; Allamandola, Louis J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Ricca, Alessandra] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
RP Mattioda, AL (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Andrew.Mattioda@nasa.gov; Charles.W.Bauschlicher@nasa.gov;
   Alessandra.Ricca-1@nasa.gov
FU NASA's Astrophysics Data Analysis Program (ADAP) [NN11AG11G]; NASA
   Astrophysics Research and Analysis Program (ARA) [10-APRA10-0167]
FX A.R. thanks the NASA's Astrophysics Data Analysis Program (ADAP)
   (NN11AG11G) for their generous support of this work. We would like to
   thank the NASA Astrophysics Research and Analysis Program (ARA)
   (10-APRA10-0167) for their generous support of this research.
NR 43
TC 3
Z9 3
U1 3
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1386-1425
J9 SPECTROCHIM ACTA A
JI Spectroc. Acta Pt. A-Molec. Biomolec. Spectr.
PD SEP 15
PY 2014
VL 130
BP 639
EP 652
DI 10.1016/j.saa.2014.04.017
PG 14
WC Spectroscopy
SC Spectroscopy
GA AL0HA
UT WOS:000338806800080
PM 24820179
ER

PT J
AU Gupta, RK
   Periyakaruppan, A
   Meyyappan, M
   Koehne, JE
AF Gupta, Rakesh K.
   Periyakaruppan, Adaikkappan
   Meyyappan, M.
   Koehne, Jessica E.
TI Label-free detection of C-reactive protein using a carbon nanofiber
   based biosensor
SO BIOSENSORS & BIOELECTRONICS
LA English
DT Article
DE Biosensors; Carbon nanofibers; C-reactive protein; Nanoelectrode array;
   Electrical impedance spectroscopy etc.
ID NANOELECTRODE ARRAYS; ELECTRODE ARRAYS; SURFACE; RISK; BIOMARKERS
AB We report the sensitive detection of C-reactive protein (CRP), a biomarker for cardiac disease, using a carbon nanofiber based biosensor platform. Vertically aligned carbon nanofibers were grown using plasma enhanced chemical vapor deposition to fabricate nanoelectrode arrays in a 3 x 3 configuration. Cyclic voltammetry (CV) and electrochemical impedance spectroscopy (EIS) were used for the CRP detection. The CV responses show a 25% reduction in redox current upon the immobilization of anti-CRP on the electrode where as a 30% increase in charge transfer resistance is seen from EIS. Further reduction in redox current and increase in charge transfer resistance result from binding of CRP on anti-CRP immobilized surface, proportional to the concentration of the CRP target. The detection limit of the sensor is found to be similar to 90 pM or similar to 11 ng/ml, which is in the clinically relevant range. Control tests using non-specific myoglobin antigen confirmed the specificity of the present approach. Published by Elsevier B.V.
C1 [Gupta, Rakesh K.; Periyakaruppan, Adaikkappan; Meyyappan, M.; Koehne, Jessica E.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Gupta, Rakesh K.] GGM Sci Coll, Dept Elect, Jammu 18004, Jammu & Kashmir, India.
   [Periyakaruppan, Adaikkappan] NASA Johnson Space Ctr, Houston, TX 77058 USA.
RP Koehne, JE (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jessica.E.Koehne@nasa.gov
FU J&K Council for science and technology, Department of Higher Education,
   JK, India; University Grants Commission (UGC), New-Delhi, India; NIH
   [R01 Ns75013]
FX JK acknowledges a Presidential Early Career Award. RKG acknowledges the
   financial support of the J&K Council for science and technology,
   Department of Higher Education, J&K, India and University Grants
   Commission (UGC), New-Delhi, India. This work was supported in part by
   NIH (R01 Ns75013).
NR 34
TC 26
Z9 26
U1 3
U2 73
PU ELSEVIER ADVANCED TECHNOLOGY
PI OXFORD
PA OXFORD FULFILLMENT CENTRE THE BOULEVARD, LANGFORD LANE, KIDLINGTON,
   OXFORD OX5 1GB, OXON, ENGLAND
SN 0956-5663
EI 1873-4235
J9 BIOSENS BIOELECTRON
JI Biosens. Bioelectron.
PD SEP 15
PY 2014
VL 59
BP 112
EP 119
DI 10.1016/j.bios.2014.03.027
PG 8
WC Biophysics; Biotechnology & Applied Microbiology; Chemistry, Analytical;
   Electrochemistry; Nanoscience & Nanotechnology
SC Biophysics; Biotechnology & Applied Microbiology; Chemistry;
   Electrochemistry; Science & Technology - Other Topics
GA AJ7CP
UT WOS:000337855100018
PM 24709327
ER

PT J
AU Hofmann, DC
   Kolodziejska, J
   Roberts, S
   Otis, R
   Dillon, RP
   Suh, JO
   Liu, ZK
   Borgonia, JP
AF Hofmann, Douglas C.
   Kolodziejska, Joanna
   Roberts, Scott
   Otis, Richard
   Dillon, Robert Peter
   Suh, Jong-Ook
   Liu, Zi-Kui
   Borgonia, John-Paul
TI Compositionally graded metals: A new frontier of additive manufacturing
SO JOURNAL OF MATERIALS RESEARCH
LA English
DT Article
ID GLASS MATRIX COMPOSITES; MICROSTRUCTURAL EVOLUTION; TENSILE DUCTILITY;
   TITANIUM-VANADIUM; LASER DEPOSITION; ALLOYS; COMPONENTS; GRADIENTS
AB The current work provides an overview of the state-of-the-art in polymer and metal additive manufacturing and provides a progress report on the science and technology behind gradient metal alloys produced through laser deposition. The research discusses a road map for creating gradient metals using additive manufacturing, demonstrates basic science results obtainable through the methodology, shows examples of prototype gradient hardware, and suggests that Compositionally Graded Metals is an emerging field of metallurgy research.
C1 [Hofmann, Douglas C.; Roberts, Scott; Dillon, Robert Peter; Suh, Jong-Ook; Borgonia, John-Paul] CALTECH, Jet Prop Lab, Engn & Sci Directorate, Pasadena, CA 91109 USA.
   [Hofmann, Douglas C.; Kolodziejska, Joanna; Roberts, Scott] CALTECH, Keck Lab Engn Sci, Pasadena, CA 91125 USA.
   [Otis, Richard; Liu, Zi-Kui] Penn State Univ, Dept Mat Sci & Engn, University Pk, PA 16802 USA.
RP Hofmann, DC (reprint author), CALTECH, Jet Prop Lab, Engn & Sci Directorate, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM dch@jpl.nasa.gov
RI Liu, Zi-Kui/A-8196-2009; 
OI Liu, Zi-Kui/0000-0003-3346-3696; Otis, Richard/0000-0002-1147-9032
FU Office of the Chief Technologist; Open Manufacturing Program of the
   Defense Advanced Research Projects Agency's Center for Innovative
   Materials Processing through Direct Digital Deposition at Penn State
   from the Office of Naval Research [N00014-12-1-0840]
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 (NASA) and funded through the
   Office of the Chief Technologist. The authors acknowledge A. Eilenberg,
   G. Agnes, A. Shapiro, C. Bradford, P. Gardner, C. Morandi, J. Mulder, P.
   Willis, and RPM Innovations for useful discussions. Richard Otis and
   Zi-Kui Liu acknowledge partial funding of this work by the Open
   Manufacturing Program of the Defense Advanced Research Projects Agency's
   Center for Innovative Materials Processing through Direct Digital
   Deposition at Penn State under Grant N00014-12-1-0840 from the Office of
   Naval Research.
NR 24
TC 8
Z9 8
U1 3
U2 52
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0884-2914
EI 2044-5326
J9 J MATER RES
JI J. Mater. Res.
PD SEP 14
PY 2014
VL 29
IS 17
SI SI
BP 1899
EP 1910
DI 10.1557/jmr.2014.208
PG 12
WC Materials Science, Multidisciplinary
SC Materials Science
GA AP6YX
UT WOS:000342225700013
ER

PT J
AU Gong, XB
   Lydon, J
   Cooper, K
   Chou, K
AF Gong, Xibing
   Lydon, James
   Cooper, Kenneth
   Chou, Kevin
TI Beam speed effects on Ti-6Al-4V microstructures in electron beam
   additive manufacturing
SO JOURNAL OF MATERIALS RESEARCH
LA English
DT Article
ID MECHANICAL-PROPERTIES; MELTED TI-6AL-4V; TITANIUM-ALLOYS; TEXTURE
AB The effect of the beam scanning speed on part microstructures in the powder-bed electron beam additive manufacturing (EBAM) process was investigated in this research. Four levels of the beam speed were tested in building EBAM Ti-6Al-4V samples. The samples were subsequently used to prepare metallographic specimens for observations by optical microscopy and scanning electron microscopy. During the experiment, a near-infrared thermal imager was also used to acquire build surface temperatures for melt tool size estimates. It was found that the X-plane (side surface) shows columnar prior beta grains, with the width in the range of about 40-110 mu m, and martensitic structures. The width of columnar grains decreases with the increase of the scanning speed. In addition, the Z-plane (scanning surface) shows equiaxed grains, in the range of 50-85 mu m. The grain size from the lowest beam speed (214 mm/s) is much larger compared to other samples of higher beam speeds (e. g., 376-689 mm/s). In addition, increasing the beam scanning speed will also result in finer a-lath. However, the porosity defect on the build surface also becomes severe at the highest scanning speed (689 mm/s).
C1 [Gong, Xibing; Chou, Kevin] Univ Alabama, Dept Mech Engn, Tuscaloosa, AL 35487 USA.
   [Lydon, James; Cooper, Kenneth] NASA, George C Marshall Space Flight Ctr, Adv Mfg Technol Team, Huntsville, AL 35812 USA.
RP Chou, K (reprint author), Univ Alabama, Dept Mech Engn, Tuscaloosa, AL 35487 USA.
EM kchou@eng.ua.edu
FU NASA [NNX11AM11A]; AL EPSCoR GRSP
FX This research is supported by NASA (award No. NNX11AM11A). Steven Price
   provided the temperature measurement results. XG also acknowledges AL
   EPSCoR GRSP for the financial support.
NR 33
TC 11
Z9 12
U1 9
U2 31
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0884-2914
EI 2044-5326
J9 J MATER RES
JI J. Mater. Res.
PD SEP 14
PY 2014
VL 29
IS 17
SI SI
BP 1951
EP 1959
DI 10.1557/jmr.2014.125
PG 9
WC Materials Science, Multidisciplinary
SC Materials Science
GA AP6YX
UT WOS:000342225700018
ER

PT J
AU Sleep, NH
   Zahnle, KJ
   Lupu, RE
AF Sleep, Norman H.
   Zahnle, Kevin J.
   Lupu, Roxana E.
TI Terrestrial aftermath of the Moon-forming impact
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL
   AND ENGINEERING SCIENCES
LA English
DT Review
DE Hadean; magma ocean; Nd-142; runaway greenhouse; CO2 subduction;
   planetary habitability
ID NUVVUAGITTUQ GREENSTONE-BELT; SMALL-SCALE CONVECTION; MAGMA OCEAN;
   THERMAL-CONVECTION; SOLAR-SYSTEM; GIANT IMPACT; SILICATE
   DIFFERENTIATION; CARBONATED ECLOGITE; DEPENDENT VISCOSITY;
   CONTINENTAL-CRUST
AB Much of the Earth's mantle was melted in the Moon-forming impact. Gases that were not partially soluble in the melt, such as water and CO2, formed a thick, deep atmosphere surrounding the post-impact Earth. This atmosphere was opaque to thermal radiation, allowing heat to escape to space only at the runaway greenhouse threshold of approximately 100 W m(-2). The duration of this runaway greenhouse stage was limited to approximately 10 Myr by the internal energy and tidal heating, ending with a partially crystalline uppermost mantle and a solid deep mantle. At this point, the crust was able to cool efficiently and solidified at the surface. After the condensation of the water ocean, approximately 100 bar of CO2 remained in the atmosphere, creating a solar-heated greenhouse, while the surface cooled to approximately 500 K. Almost all this CO2 had to be sequestered by subduction into the mantle by 3.8 Ga, when the geological record indicates the presence of life and hence a habitable environment. The deep CO2 sequestration into the mantle could be explained by a rapid subduction of the old oceanic crust, such that the top of the crust would remain cold and retain its CO2. Kinematically, these episodes would be required to have both fast subduction (and hence seafloor spreading) and old crust. Hadean oceanic crust that formed from hot mantle would have been thicker than modern crust, and therefore only old crust underlain by cool mantle lithosphere could subduct. Once subduction started, the basaltic crust would turn into dense eclogite, increasing the rate of subduction. The rapid subduction would stop when the young partially frozen crust from the rapidly spreading ridge entered the subduction zone.
C1 [Sleep, Norman H.] Stanford Univ, Dept Geophys, Stanford, CA 94305 USA.
   [Zahnle, Kevin J.; Lupu, Roxana E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Sleep, NH (reprint author), Stanford Univ, Dept Geophys, Stanford, CA 94305 USA.
EM norm@stanford.edu
RI Lupu, Roxana/P-9060-2014
OI Lupu, Roxana/0000-0003-3444-5908
NR 105
TC 9
Z9 9
U1 5
U2 49
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1364-503X
EI 1471-2962
J9 PHILOS T R SOC A
JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci.
PD SEP 13
PY 2014
VL 372
IS 2024
AR 20130172
DI 10.1098/rsta.2013.0172
PG 26
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AN7RY
UT WOS:000340799400002
PM 25114303
ER

PT J
AU Bauschlicher, CW
   Haskins, JB
   Bucholz, EW
   Lawson, JW
   Borodin, O
AF Bauschlicher, Charles W., Jr.
   Haskins, Justin B.
   Bucholz, Eric W.
   Lawson, John W.
   Borodin, Oleg
TI Structure and Energetics of Li+-(BF4-)(n ') Li+-(FSI-)(n '), and
   Li+-(TFSI-)(n): Ab Initio and Polarizable Force Field Approaches
SO JOURNAL OF PHYSICAL CHEMISTRY B
LA English
DT Article
ID MOLECULAR-DYNAMICS SIMULATIONS; MAIN-GROUP THERMOCHEMISTRY;
   GAUSSIAN-BASIS SETS; NONCOVALENT INTERACTIONS; IONIC LIQUIDS; ELECTRON
   CORRELATION; LITHIUM BATTERIES; EXCHANGE; KINETICS; APPROXIMATION
AB The Li+-BF4- and BF4--BF4- interactions are studied using second order perturbation theory (MP2) and coupled cluster singles and doubles approach, including the effect of connected triples, CCSD(T). The MP2 and CCSD(T) results are in excellent agreement. Using only the MP2 approach, the interactions of Li+ with bis(trifluoromethane)sulfonimide anion (TFSI) and Li+ with bis(fluorosulfonyl)imide anion (FSI) are studied. The results of these high level calculations are compared with density functional theory (DFT) calculations for a variety of functionals and with the APPLE&P force field. The B3LYP approach well reproduces the accurate calculations using both a small and large basis set. The M06 and M06L functionals in the larger basis set are in good agreement with the high level calculations. While the APPLE&P force field does not outperform the best functionals, the APPLE&P results agree better with the accurate results than do some of the functionals tested.
C1 [Bauschlicher, Charles W., Jr.; Haskins, Justin B.; Bucholz, Eric W.; Lawson, John W.; Borodin, Oleg] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Borodin, Oleg] US Army Res Lab, Sensor & Electron Devices Directorate, Electrochem Branch, Adelphi, MD 20783 USA.
EM Charles.W.Bauschlicher@nasa.gov
RI Borodin, Oleg/B-6855-2012
OI Borodin, Oleg/0000-0002-9428-5291
FU NASA Aeronautics Research Institute Seedling program
FX This work was supported by funding from the NASA Aeronautics Research
   Institute Seedling program.
NR 31
TC 9
Z9 9
U1 3
U2 30
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1520-6106
J9 J PHYS CHEM B
JI J. Phys. Chem. B
PD SEP 11
PY 2014
VL 118
IS 36
BP 10785
EP 10794
DI 10.1021/jp506422p
PG 10
WC Chemistry, Physical
SC Chemistry
GA AO8QP
UT WOS:000341619600024
PM 25180695
ER

PT J
AU Satyal, S
   Hinse, TC
   Quarles, B
   Noyola, JP
AF Satyal, S.
   Hinse, T. C.
   Quarles, B.
   Noyola, J. P.
TI Chaotic dynamics of the planet in HD 196885 AB
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: numerical; celestial mechanics; binaries: general; stars:
   individual: HD 196885; planetary systems
ID HIERARCHICAL 3-BODY SYSTEMS; BINARY STAR SYSTEMS; HOT JUPITERS; KOZAI
   MECHANISM; EXTRASOLAR PLANETS; STELLAR BINARIES; GLOBAL DYNAMICS;
   EVOLUTION; ECCENTRICITY; STABILITY
AB Depending on the planetary orbit around the host star(s), a planet could orbit either one or both stars in a binary system as S type or P type, respectively. We have analysed the dynamics of the S-type planetary system in HD 196885 AB with an emphasis on a planet with a higher orbital inclination relative to the binary plane. The mean exponential growth factor of nearby orbits (MEGNO) maps are used as an indicator to determine regions of periodicity and chaos for the various choices of the planet's semimajor axis, eccentricity and inclination with respect to the previously determined observational uncertainties. We have quantitatively mapped out the chaotic and quasi-periodic regions of the system's phase space which indicate a likely regime of the planet's inclination. In addition, we inspect the resonant angle to determine whether alternation between libration and circulation occurs as a consequence of Kozai oscillations, a probable mechanism that can drive the planetary orbit to a very large inclination. Also, we demonstrate the possible higher mass limit of the planet and improve upon the current dynamical model based on our analysis.
C1 [Satyal, S.; Noyola, J. P.] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA.
   [Hinse, T. C.] Korea Astron & Space Sci Inst, Taejon 304358, South Korea.
   [Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland.
   [Quarles, B.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div 245 3, Moffett Field, CA 94035 USA.
RP Satyal, S (reprint author), Univ Texas Arlington, Dept Phys, POB 19059, Arlington, TX 76019 USA.
EM ssatyal@uta.edu
FU NASA; Korea Research Council for Fundamental Science and Technology
   (KRCF) through the Young Research Scientist Fellowship Program; KASI
   (Korea Astronomy and Space Science Institute) [2014-1-400-06]; Northern
   Ireland Department of Culture, Arts and Leisure (DCAL)
FX SS and JN would like to thank The Department of Physics at UT Arlington,
   Zdzislaw Musielak and Manfred Cuntz for their continuous support and
   guidance. BQ gratefully acknowledges support from the NASA post-doctoral
   programme. TCH 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
   2014-1-400-06. Numerical computations were partly carried out using the
   SFI/HEA Irish Centre for High-End Computing (ICHEC) and the PLUTO
   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). We
   would also like to thank the anonymous referee for his/her comments and
   suggestions on eccentric Lidov-Kozai mechanism which significantly
   improved this work.
NR 48
TC 3
Z9 3
U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 11
PY 2014
VL 443
IS 2
BP 1310
EP 1318
DI 10.1093/mnras/stu1221
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AN2SY
UT WOS:000340436800028
ER

PT J
AU Parker, ML
   Wilkins, DR
   Fabian, AC
   Grupe, D
   Dauser, T
   Matt, G
   Harrison, FA
   Brenneman, L
   Boggs, SE
   Christensen, FE
   Craig, WW
   Gallo, LC
   Hailey, CJ
   Kara, E
   Komossa, S
   Marinucci, A
   Miller, JM
   Risaliti, G
   Stern, D
   Walton, DJ
   Zhang, WW
AF Parker, M. L.
   Wilkins, D. R.
   Fabian, A. C.
   Grupe, D.
   Dauser, T.
   Matt, G.
   Harrison, F. A.
   Brenneman, L.
   Boggs, S. E.
   Christensen, F. E.
   Craig, W. W.
   Gallo, L. C.
   Hailey, C. J.
   Kara, E.
   Komossa, S.
   Marinucci, A.
   Miller, J. M.
   Risaliti, G.
   Stern, D.
   Walton, D. J.
   Zhang, W. W.
TI The NuSTAR spectrum of Mrk 335: extreme relativistic effects within two
   gravitational radii of the event horizon?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: individual: Mrk 335; galaxies: Seyfert
ID ACTIVE GALACTIC NUCLEI; X-RAY REFLECTION; ACCRETING BLACK-HOLES;
   XMM-NEWTON; FLUX STATE; LONG HARD; NGC 4051; IRAS 13224-3809;
   EMISSION-LINES; 1H 0707-495
AB We present 3-50 keV NuSTAR observations of the active galactic nuclei Mrk 335 in a very low flux state. The spectrum is dominated by very strong features at the energies of the iron line at 5-7 keV and Compton hump from 10-30 keV. The source is variable during the observation, with the variability concentrated at low energies, which suggesting either a relativistic reflection or a variable absorption scenario. In this work, we focus on the reflection interpretation, making use of new relativistic reflection models that self consistently calculate the reflection fraction, relativistic blurring and angle-dependent reflection spectrum for different coronal heights to model the spectra. We find that the spectra can be well fitted with relativistic reflection, and that the lowest flux state spectrum is described by reflection alone, suggesting the effects of extreme light-bending occurring within similar to 2 gravitational radii (R-G) of the event horizon. The reflection fraction decreases sharply with increasing flux, consistent with a point source moving up to above 10 R-G as the source brightens. We constrain the spin parameter to greater than 0.9 at the 3 sigma confidence level. By adding a spin-dependent upper limit on the reflection fraction to our models, we demonstrate that this can be a powerful way of constraining the spin parameter, particularly in reflection dominated states. We also calculate a detailed emissivity profile for the iron line, and find that it closely matches theoretical predictions for a compact source within a few R-G of the black hole.
C1 [Parker, M. L.; Wilkins, D. R.; Fabian, A. C.; Kara, E.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
   [Wilkins, D. R.; Gallo, L. C.] St Marys Univ, Halifax, NS B3H 3C3, Canada.
   [Grupe, D.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
   [Dauser, T.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany.
   [Dauser, T.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany.
   [Matt, G.; Marinucci, A.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy.
   [Harrison, F. A.; Walton, D. J.] CALTECH, Pasadena, CA 91125 USA.
   [Brenneman, L.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
   [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA.
   [Craig, W. W.; Hailey, C. J.] Columbia Univ, New York, NY 10027 USA.
   [Komossa, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
   [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
   [Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
   [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Parker, ML (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
EM mlparker@ast.cam.ac.uk
RI Boggs, Steven/E-4170-2015; 
OI Boggs, Steven/0000-0001-9567-4224; Risaliti, Guido/0000-0002-3556-977X
FU NASA [NAS5-00136]; Science and Technology Facilities Council (STFC);
   Royal Society; Italian Space Agency [ASI/INAFI/037/12/0 - 011/13]; CITA
   National Fellowship; European Union [312789]
FX This work is based on observations made by the NuSTAR mission, a project
   led by the California Institute of Astronomy, managed by the Jet
   Propulsion Laboratory, and funded by NASA. This research has made use of
   the NUSTARDAS, jointly developed by the ASI Science Data Center (ASDC,
   Italy) and the California Institute of Technology (USA). At Penn State
   Swift is supported by NASA contract NAS5-00136. MLP acknowledges
   financial support from the Science and Technology Facilities Council
   (STFC). ACF thanks the Royal Society for support. AM and GM acknowledge
   financial support from Italian Space Agency under grant
   ASI/INAFI/037/12/0 - 011/13. DRW is supported by a CITA National
   Fellowship. The research leading to these results has received funding
   from the European Union Seventh Framework Programme (FP7/2007-2013)
   under grant agreement no. 312789.
NR 57
TC 37
Z9 37
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 11
PY 2014
VL 443
IS 2
BP 1723
EP 1732
DI 10.1093/mnras/stu1246
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AN2SY
UT WOS:000340436800062
ER

PT J
AU Bellm, EC
   Furst, F
   Pottschmidt, K
   Tomsick, JA
   Boggs, SE
   Chakrabarty, D
   Christensen, FE
   Craig, WW
   Hailey, CJ
   Harrison, FA
   Stern, D
   Walton, DJ
   Wilms, J
   Zhang, WW
AF Bellm, Eric C.
   Fuerst, Felix
   Pottschmidt, Katja
   Tomsick, John A.
   Boggs, Steven E.
   Chakrabarty, Deepto
   Christensen, Finn E.
   Craig, William W.
   Hailey, Charles J.
   Harrison, Fiona A.
   Stern, Daniel
   Walton, Dominic J.
   Wilms, Joern
   Zhang, William W.
TI CONFIRMATION OF A HIGH MAGNETIC FIELD IN GRO J1008-57
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (GRO J1008-57); stars: neutron; X-rays: binaries
ID SPECTROSCOPIC-TELESCOPE-ARRAY; X-RAY PULSARS; CYCLOTRON LINE; LMC X-4;
   ENERGY; ABSORPTION; DISCOVERY; SPECTRUM; MISSION; BINARY
AB GRO J1008-57 is a high-mass X-ray binary for which several claims of a cyclotron resonance scattering feature near 80 keV have been reported. We use NuSTAR, Suzaku, and Swift data from its giant outburst of 2012 November to confirm the existence of the 80 keV feature and perform the most sensitive search to date for cyclotron scattering features at lower energies. We find evidence for a 78(-2)(+3) keV line in the NuSTAR and Suzaku data at >4 sigma significance, confirming the detection using Suzaku alone by Yamamoto et al. A search of both the phase-averaged and phase-resolved data rules out a fundamental at lower energies with optical depth larger than 5% of the 78 keV line. These results indicate that GRO J1008-57 has a magnetic field of 6.7 x 10(12)(1 + z) G, the highest among known accreting pulsars.
C1 [Bellm, Eric C.; Fuerst, Felix; Harrison, Fiona A.; Walton, Dominic J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
   [Pottschmidt, Katja] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
   [Pottschmidt, Katja] CRESST, Greenbelt, MD 20771 USA.
   [Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
   [Tomsick, John A.; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
   [Christensen, Finn E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark.
   [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
   [Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Wilms, Joern] Dr Karl Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany.
   [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Bellm, EC (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
EM ebellm@caltech.edu
RI Wilms, Joern/C-8116-2013; Boggs, Steven/E-4170-2015; XRAY,
   SUZAKU/A-1808-2009
OI Wilms, Joern/0000-0003-2065-5410; Boggs, Steven/0000-0001-9567-4224; 
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
   Deutsches Zentrum fur Luftund Raumfahrt [50 OR 1113]
FX This work was supported under NASA contract No. NNG08FD60C and uses data
   from the NuSTAR mission, a project led by the California Institute of
   Technology, managed by the Jet Propulsion Laboratory, and funded by the
   National Aeronautics and Space Administration. We thank the NuSTAR
   Operations team for executing the ToO observation and the Software and
   Calibration teams for analysis support. This research has used the
   NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI
   Science Data Center (ASDC, Italy) and the California Institute of
   Technology (USA). J.W. acknowledges partial support from Deutsches
   Zentrum fur Luftund Raumfahrt grant 50 OR 1113.
NR 41
TC 3
Z9 3
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2014
VL 792
IS 2
AR 108
DI 10.1088/0004-637X/792/2/108
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RF
UT WOS:000341172200026
ER

PT J
AU Burlaga, LF
   Ness, NF
   Florinski, V
   Heerikhuisen, J
AF Burlaga, L. F.
   Ness, N. F.
   Florinski, V.
   Heerikhuisen, J.
TI MAGNETIC FIELD FLUCTUATIONS OBSERVED IN THE HELIOSHEATH AND INTERSTELLAR
   MAGNETIC FIELD BY VOYAGER 1 AT 115.7-124.9 AU DURING 2011-2013
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instabilities; ISM: kinematics and dynamics; solar wind; turbulence
ID BOUNDARY-EXPLORER RIBBON; COSMIC-RAY MODULATION; SOLAR-WIND; OUTER
   HELIOSPHERE; TERMINATION SHOCK; IBEX RIBBON; HELIOPAUSE; TURBULENCE;
   TRANSPORT; IONS
AB We discuss microscale fluctuations of the hour averages of the magnetic field B observed on a scale of one day by Voyager 1 (V1) from 2011.0 to 2012.3143 (when it was within the distant heliosheath, where the average magnetic field strength < B > = 0.17 nT) and during the interval from 2012.6503 to 2013.5855 (when it was within the interstellar plasma with < B > = 0.47 nT). In both regions, the fluctuations were primarily compressive fluctuations, varying along the average B (approximate to T direction in RTN coordinates). In the heliosheath, the average of the daily standard deviations (SDs) of the compressive and transverse components of B were < SDc > = 0.010 nT and < SDt > <= 0.005 nT (which is the limit of the measurement). In the distant heliosheath < SDc >/< B > = 0.06, and the distributions of SD were skewed and highly kurtotic. The interstellar magnetic field (ISMF) strength was B = 0.48 nT, but the fluctuations were below the limit of measurement: < SDc > = 0.004 nT and < abs(SDt)> = 0.004 nT. The distributions of these interstellar SDs have skewness and kurtosis consistent with a Gaussian noise distribution. We also discuss the fluctuations of 48 s averages of B on a scale of 1 day during a 30 day interval when V1 was observing the ISMF. For the fluctuations in all three components of B, SD = 0.010 nT, which gives an upper limit on the fluctuations of the ISMF on the scales observed by V1. This SD rules out the possibility that there is significant power in electromagnetic fluctuations generated by pickup ion ring instabilities at these scales, which strongly constrains models of the IBEX ribbon.
C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
   [Florinski, V.; Heerikhuisen, J.] Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA.
RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Code 673, Greenbelt, MD 20771 USA.
EM lburlagahsp@verizon.net; nfnudel@yahoo.com
OI Heerikhuisen, Jacob/0000-0001-7867-3633
FU NASA [NASA NNX 12AC63G, NASA NNX 14AB61A]
FX Daniel Berdichevsky computed the zero level offsets for the instrument.
   The data were processed by T. McClanahan and S. Kramer. N. F. Ness was
   partially supported by NASA grants NASA NNX 12AC63G and NASA NNX 14AB61A
   to the Catholic University of America.
NR 53
TC 10
Z9 10
U1 0
U2 9
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 2014
VL 792
IS 2
AR 134
DI 10.1088/0004-637X/792/2/134
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RF
UT WOS:000341172200052
ER

PT J
AU David, LP
   Lim, J
   Forman, W
   Vrtilek, J
   Combes, F
   Salome, P
   Edge, A
   Hamer, S
   Jones, C
   Sun, M
   O'Sullivan, E
   Gastaldello, F
   Bardelli, S
   Temi, P
   Schmitt, H
   Ohyama, Y
   Mathews, W
   Brighenti, F
   Giacintucci, S
   Trung, DV
AF David, Laurence P.
   Lim, Jeremy
   Forman, William
   Vrtilek, Jan
   Combes, Francoise
   Salome, Philippe
   Edge, Alastair
   Hamer, Stephen
   Jones, Christine
   Sun, Ming
   O'Sullivan, Ewan
   Gastaldello, Fabio
   Bardelli, Sandro
   Temi, Pasquale
   Schmitt, Henrique
   Ohyama, Youichi
   Mathews, William
   Brighenti, Fabrizio
   Giacintucci, Simona
   Trung, Dinh-V
TI MOLECULAR GAS IN THE X-RAY BRIGHT GROUP NGC 5044 AS REVEALED BY ALMA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: clusters: general; galaxies: groups:
   individual (NGC 5044); galaxies: ISM
ID EARLY-TYPE GALAXIES; GALACTIC NUCLEUS FEEDBACK; CENTRAL CLUSTER
   GALAXIES; COOLING FLOW CLUSTERS; STAR-FORMATION; ELLIPTIC GALAXIES;
   TELESCOPE OBSERVATIONS; SPITZER OBSERVATIONS; LUMINOUS CLUSTERS;
   HIGH-RESOLUTION
AB An ALMA observation of the early-type galaxy NGC 5044, which resides at the center of an X-ray bright group with a moderate cooling flow, detected 24 molecular structures within the central 2.5 kpc. The masses of the molecular structures vary from 3 x 10(5) M-circle dot to 10(7) M-circle dot and the CO(2-1) linewidths vary from 15 to 65 km s(-1). Given the large CO(2-1) linewidths, the observed structures are likely giant molecular associations (GMAs) and not individual giant molecular clouds (GMCs). Only a few of the GMAs are spatially resolved and the average density of these GMAs yields a GMC volume filling factor of about 15%. The masses of the resolved GMAs are insufficient for them to be gravitationally bound, however, the most massive GMA does contain a less massive component with a linewidth of 5.5 km s(-1) (typical of an individual virialized GMC). We also show that the GMAs cannot be pressure confined by the hot gas. Given the CO(2-1) linewidths of the GMAs (i.e., the velocity dispersion of the embedded GMCs) they should disperse on a timescale of about 12 Myr. No disk-like molecular structures are detected and all indications suggest that the molecular gas follows ballistic trajectories after condensing out of the thermally unstable hot gas. The 230 GHz luminosity of the central continuum source is 500 times greater than its low frequency radio luminosity and probably reflects a recent accretion event. The spectrum of the central continuum source also exhibits an absorption feature with a linewidth typical of an individual GMC and an infalling velocity of 250 km s(-1).
C1 [David, Laurence P.; Forman, William; Vrtilek, Jan; Jones, Christine; O'Sullivan, Ewan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Lim, Jeremy] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
   [Combes, Francoise; Salome, Philippe] CNRS, Observ Paris, LERMA, F-75014 Paris, France.
   [Edge, Alastair; Hamer, Stephen] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England.
   [Sun, Ming] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
   [Gastaldello, Fabio; Bardelli, Sandro] IASF Milano, INAF, I-20133 Milan, Italy.
   [Temi, Pasquale] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
   [Schmitt, Henrique] Naval Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
   [Ohyama, Youichi] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan.
   [Mathews, William] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Brighenti, Fabrizio] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
   [Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Trung, Dinh-V] Vietnamese Acad Sci & Technol, Inst Phys, Hanoi, Vietnam.
RP David, LP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ldavid@head.cfa.harvard.edu
RI Gastaldello, Fabio/N-4226-2015; Bardelli, Sandro/O-9369-2015; 
OI Gastaldello, Fabio/0000-0002-9112-0184; Bardelli,
   Sandro/0000-0002-8900-0298; O'Sullivan, Ewan/0000-0002-5671-6900; Edge,
   Alastair/0000-0002-3398-6916; Forman, William/0000-0002-9478-1682;
   Combes, Francoise/0000-0003-2658-7893
FU NASA [GO2-13146X]; STFC [ST/I001573/1]
FX This paper makes use of the following ALMA data:
   ADS/JAO.ALMA#2011.0.00735. S. ALMA is a partnership of ESO (representing
   its member states), NSF (USA), and NINS (Japan), together with NRC
   (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of
   Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and
   NAOJ. The National Radio Astronomy Observatory is a facility of the
   National Science Foundation operated under cooperative agreement by
   Associated Universities, Inc. This work was supported in part by NASA
   grant GO2-13146X. A.C.E. acknowledges support from STFC grant
   ST/I001573/1. We thank M. Birkinshaw for assistance in learning CASA and
   analyzing the ALMA data and B. McNamara and P. Nulsen for discussions
   about their cycle 0 ALMA observations of clusters of galaxies.
NR 64
TC 13
Z9 13
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 2014
VL 792
IS 2
AR 94
DI 10.1088/0004-637X/792/2/94
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RF
UT WOS:000341172200012
ER

PT J
AU Degenaar, N
   Wijnands, R
   Reynolds, MT
   Miller, JM
   Altamirano, D
   Kennea, J
   Gehrels, N
   Haggard, D
   Ponti, G
AF Degenaar, N.
   Wijnands, R.
   Reynolds, M. T.
   Miller, J. M.
   Altamirano, D.
   Kennea, J.
   Gehrels, N.
   Haggard, D.
   Ponti, G.
TI THE PECULIAR GALACTIC CENTER NEUTRON STAR X-RAY BINARY XMM
   J174457-2850.3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; Galaxy: center; pulsars: general; stars:
   neutron; X-rays: binaries; X-rays: individual (XMM J174457-2850.3)
ID DISC INSTABILITY MODEL; PHOTON IMAGING CAMERA; SYSTEM PSR J1023+0038;
   MILLISECOND PULSAR; XSS J12270-4859; QUIESCENT STATE; RADIO PULSARS; SAX
   J1808.4-3658; CENTER REGION; TRANSIENTS
AB The recent discovery of a millisecond radio pulsar experiencing an accretion outburst similar to those seen in low mass X-ray binaries, has opened up a new opportunity to investigate the evolutionary link between these two different neutron star manifestations. The remarkable X-ray variability and hard X-ray spectrum of this object can potentially serve as a template to search for other X-ray binary/radio pulsar transitional objects. Here we demonstrate that the transient X-ray source XMM J174457-2850.3 near the Galactic center displays similar X-ray properties. We report on the detection of an energetic thermonuclear burst with an estimated duration of similar or equal to 2 hr and a radiated energy output of similar or equal to 5 x 10(40) erg, which unambiguously demonstrates that the source harbors an accreting neutron star. It has a quiescent X-ray luminosity of L-X similar or equal to 5 x 10(32)(D/6.5 kpc)(2) erg s(-1) and exhibits occasional accretion outbursts during which it brightens to LX similar or equal to 10(35)- 10(36)(D/6.5 kpc)(2) erg s(-1) for a few weeks (2-10 keV). However, the source often lingers in between outburst and quiescence at L-X similar or equal to 10(33)- 10(34)(D/6.5 kpc)(2) erg s(-1). This peculiar X-ray flux behavior and its relatively hard X-ray spectrum, a power law with an index of Gamma similar or equal to 1.4, could possibly be explained in terms of the interaction between the accretion flow and the magnetic field of the neutron star.
C1 [Degenaar, N.; Reynolds, M. T.; Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
   [Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
   [Altamirano, D.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
   [Kennea, J.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
   [Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
   [Haggard, D.] Northwestern Univ, CIERA, Dept Phys & Astron, Evanston, IL 60208 USA.
   [Ponti, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
RP Degenaar, N (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
EM degenaar@umich.edu
FU NASA from Space Telescope Science Institute [HST-HF-51287.01-A]; Royal
   Society; EU Marie Curie Intra-European Fellowship
   [EFP7-PEOPLE-2012-IEF-331095]
FX N.D. is supported by NASA through Hubble Postdoctoral Fellowship grant
   number HST-HF-51287.01-A from the Space Telescope Science Institute,
   which is operated by the Association of Universities for Research in
   Astronomy, Incorporated, under NASA contract NAS5-26555. D.A.
   acknowledges support from the Royal Society. G.P. is supported by an EU
   Marie Curie Intra-European Fellowship under contract number
   EFP7-PEOPLE-2012-IEF-331095. This work made use of the public data
   archives of Swift, Chandra, and XMM-Newton.
NR 96
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 2014
VL 792
IS 2
AR 109
DI 10.1088/0004-637X/792/2/109
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RF
UT WOS:000341172200027
ER

PT J
AU Domagal-Goldman, SD
   Segura, A
   Claire, MW
   Robinson, TD
   Meadows, VS
AF Domagal-Goldman, Shawn D.
   Segura, Antigona
   Claire, Mark W.
   Robinson, Tyler D.
   Meadows, Victoria S.
TI ABIOTIC OZONE AND OXYGEN IN ATMOSPHERES SIMILAR TO PREBIOTIC EARTH
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Earth; infrared: planetary systems; planets and satellites: atmospheres;
   planets and satellites: terrestrial planets; planet-star interactions;
   ultraviolet: planetary systems
ID MAIN-SEQUENCE STARS; LOW-MASS STARS; M-DWARFS; TERRESTRIAL PLANETS;
   EXTRASOLAR PLANETS; HABITABLE ZONES; WATER-VAPOR; AD LEONIS; MARS;
   EXOPLANET
AB The search for life on planets outside our solar system will use spectroscopic identification of atmospheric biosignatures. The most robust remotely detectable potential biosignature is considered to be the detection of oxygen (O-2) or ozone (O-3) simultaneous to methane (CH4) at levels indicating fluxes from the planetary surface in excess of those that could be produced abiotically. Here we use an altitude-dependent photochemical model with the enhanced lower boundary conditions necessary to carefully explore abiotic O-2 and O-3 production on lifeless planets with a wide variety of volcanic gas fluxes and stellar energy distributions. On some of these worlds, we predict limited O-2 and O-3 buildup, caused by fast chemical production of these gases. This results in detectable abiotic O-3 and CH4 features in the UV-visible, but no detectable abiotic O-2 features. Thus, simultaneous detection of O-3 and CH4 by a UV-visible mission is not a strong biosignature without proper contextual information. Discrimination between biological and abiotic sources of O-2 and O-3 is possible through analysis of the stellar and atmospheric context-particularly redox state and O atom inventory-of the planet in question. Specifically, understanding the spectral characteristics of the star and obtaining a broad wavelength range for planetary spectra should allow more robust identification of false positives for life. This highlights the importance of wide spectral coverage for future exoplanet characterization missions. Specifically, discrimination between true and false positives may require spectral observations that extend into infrared wavelengths and provide contextual information on the planet's atmospheric chemistry.
C1 [Domagal-Goldman, Shawn D.] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA.
   [Domagal-Goldman, Shawn D.; Segura, Antigona; Claire, Mark W.; Robinson, Tyler D.; Meadows, Victoria S.] NASA, Astrobiol Inst, Virtual Planetary Lab, Washington, DC USA.
   [Segura, Antigona] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04530, DF, Mexico.
   [Claire, Mark W.] Univ St Andrews, Dept Earth & Environm Sci, St Andrews KY16 9AL, Fife, Scotland.
   [Robinson, Tyler D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Meadows, Victoria S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
RP Domagal-Goldman, SD (reprint author), NASA, Goddard Space Flight Ctr, Planetary Environm Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM shawn.goldman@nasa.gov
FU National Aeronautics and Space Administration through the NASA
   Astrobiology Institute [NNH05ZDA001C]; Oak Ridge Associated Universities
   NASA Postdoctoral Program
FX 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 No. NNH05ZDA001C. S.D.D.-G., M.W.C., and T.D.R. acknowledge
   additional support from the Oak Ridge Associated Universities NASA
   Postdoctoral Program; S.D.D.-G. did much of the work on this project
   while an NPP Management Fellow in residence at NASA Headquarters, M.W.C.
   while in residence at the University of Washington, and T.D.R. while in
   residence at NASA Ames.
NR 84
TC 34
Z9 34
U1 5
U2 40
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 2014
VL 792
IS 2
AR 90
DI 10.1088/0004-637X/792/2/90
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RF
UT WOS:000341172200008
ER

PT J
AU Gandhi, P
   Lansbury, GB
   Alexander, DM
   Stern, D
   Arevalo, P
   Ballantyne, DR
   Balokovic, M
   Bauer, FE
   Boggs, SE
   Brandt, WN
   Brightman, M
   Christensen, FE
   Comastri, A
   Craig, WW
   Del Moro, A
   Elvis, M
   Fabian, AC
   Hailey, CJ
   Harrison, FA
   Hickox, RC
   Koss, M
   LaMassa, SM
   Luo, B
   Madejski, GM
   Ptak, AF
   Puccetti, S
   Teng, SH
   Urry, CM
   Walton, DJ
   Zhang, WW
AF Gandhi, P.
   Lansbury, G. B.
   Alexander, D. M.
   Stern, D.
   Arevalo, P.
   Ballantyne, D. R.
   Balokovic, M.
   Bauer, F. E.
   Boggs, S. E.
   Brandt, W. N.
   Brightman, M.
   Christensen, F. E.
   Comastri, A.
   Craig, W. W.
   Del Moro, A.
   Elvis, M.
   Fabian, A. C.
   Hailey, C. J.
   Harrison, F. A.
   Hickox, R. C.
   Koss, M.
   LaMassa, S. M.
   Luo, B.
   Madejski, G. M.
   Ptak, A. F.
   Puccetti, S.
   Teng, S. H.
   Urry, C. M.
   Walton, D. J.
   Zhang, W. W.
TI NuSTAR UNVEILS A COMPTON-THICK TYPE 2 QUASAR IN MrK 34
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; X-rays: galaxies; X-rays: individual (Mrk 34)
ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; SEYFERT 2 GALAXIES;
   X-RAY-EMISSION; STAR-FORMING GALAXIES; NARROW-LINE REGION; XMM-NEWTON
   SURVEY; BLACK-HOLE MASS; SWIFT-BAT SURVEY; MIDINFRARED SELECTION
AB We present Nuclear Spectroscopic Telescope Array (NuSTAR) 3-40 keV observations of the optically selected Type 2 quasar (QSO2) SDSS J1034+6001 or Mrk 34. The high-quality hard X-ray spectrum and archival XMM-Newton data can be fitted self-consistently with a reflection-dominated continuum and a strong Fe K alpha fluorescence line with equivalent width > 1 keV. Prior X-ray spectral fitting below 10 keV showed the source to be consistent with being obscured by Compton-thin column densities of gas along the line of sight, despite evidence for much higher columns from multiwavelength data. NuSTAR now enables a direct measurement of this column and shows that N-H lies in the Compton-thick (CT) regime. The new data also show a high intrinsic 2-10 keV luminosity of L2-10 similar to 10(44) erg s (1), in contrast to previous low-energy X-ray measurements where L2-10 less than or similar to 10(43) erg s (1) (i.e., X-ray selection below 10 keV does not pick up this source as an intrinsically luminous obscured quasar). Both the obscuring column and the intrinsic power are about an order of magnitude (or more) larger than inferred from pre-NuSTAR X-ray spectral fitting. Mrk 34 is thus a "gold standard" CT QSO2 and is the nearest non-merging system in this class, in contrast to the other local CT quasar NGC 6240, which is currently undergoing a major merger coupled with strong star formation. For typical X-ray bolometric correction factors, the accretion luminosity of Mrk 34 is high enough to potentially power the total infrared luminosity. X-ray spectral fitting also shows that thermal emission related to star formation is unlikely to drive the observed bright soft component below similar to 3 keV, favoring photoionization instead.
C1 [Gandhi, P.; Lansbury, G. B.; Alexander, D. M.; Del Moro, A.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
   [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Arevalo, P.; Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Spain.
   [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile.
   [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
   [Balokovic, M.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
   [Bauer, F. E.] Millennium Inst Astrophys, Santiago, Chile.
   [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
   [Boggs, S. E.; Luo, B.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
   [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
   [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
   [Brightman, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
   [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark.
   [Comastri, A.] INAF Osserv Astron Bologna, I-40127 Bologna, Italy.
   [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
   [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
   [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
   [Hickox, R. C.] Dartmouth Coll, Wilder Lab 6127, Dept Phys & Astron, Hanover, NH 03755 USA.
   [Koss, M.] Swiss Fed Inst Technol, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland.
   [LaMassa, S. M.; Urry, C. M.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
   [Madejski, G. M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
   [Ptak, A. F.; Zhang, W. W.] NASA Goddard Space Flight Ctr, XRay Astrophys Lab, Greenbelt, MD 20771 USA.
   [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy.
   [Puccetti, S.] INAF Osserv Astron Roma, I-00040 Monte Porzio Catone, RM, Italy.
   [Teng, S. H.] NASA Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
RP Gandhi, P (reprint author), Univ Durham, Dept Phys, Durham DH1 3LE, England.
RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt,
   William/N-2844-2015; Comastri, Andrea/O-9543-2015; 
OI Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581;
   Brandt, William/0000-0002-0167-2453; Comastri,
   Andrea/0000-0003-3451-9970; Puccetti, Simonetta/0000-0002-2734-7835;
   Urry, Meg/0000-0002-0745-9792
FU STFC [ST/J003697/1, ST/K501979/1, ST/I001573/1]; Leverhulme Trust; NASA
   Postdoctoral Program; ASI-INAF grant; Anillo [ACT1101]; FONDECYT
   [1140304]; International Fulbright Science and Technology Award; Swiss
   National Science Foundation (NSF) [PP00P2 138979/1]; Durham University
   COFUND fellowship; Basal-CATA [PFB-06/2007]; CONICYT-Chile (FONDECYT
   [1141218]; "EMBIGGEN" Anillo [ACT1101]; Iniciativa Cientifica Milenio
   del Ministerio de Economia, Fomento y Turismo [IC120009]; National
   Aeronautics and Space Administration (NASA); NuSTAR Operations,
   Software, and Calibration teams
FX Grant and fellowship acknowledgments: STFC ST/J003697/1 (P.G.),
   ST/K501979/1 (G.B.L.), ST/I001573/1 (D.M.A. and A.D.M.), Leverhulme
   Trust (D.M.A.), NASA Postdoctoral Program (S.H.T), ASI-INAF grant
   (A.C.), Anillo ACT1101 and FONDECYT 1140304 (P.A.), International
   Fulbright Science and Technology Award (M. B.), and Swiss National
   Science Foundation (NSF) grant PP00P2 138979/1 (M.K.). In addition,
   F.A.H. acknowledges support from a Durham University COFUND fellowship,
   and F.E.B. acknowledges support from Basal-CATA PFB-06/2007,
   CONICYT-Chile (FONDECYT 1141218 and "EMBIGGEN" Anillo ACT1101) Project
   IC120009 "Millennium Institute of Astrophysics (MAS)" funded by the
   Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y
   Turismo. The authors thank Fred K.Y. Lo for megamaser discussions, and
   the referee for the report. P.G. thanks James R. Mullaney and Chris M.
   Harrison for discussions. P.G. is also grateful to Matteo Guainazzi for
   his comments and insights on the origin of the soft X-ray spectrum.;
   NuSTAR is a project led by the California Institute of Technology
   (Caltech), managed by the Jet Propulsion Laboratory (JPL), and funded by
   the National Aeronautics and Space Administration (NASA). The NuSTAR
   Operations, Software, and Calibration teams are acknowledged for support
   with these observations. This research has made use of the NuSTAR Data
   Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data
   Center (ASDC, Italy) and the California Institute of Technology (USA).
   This work has made use of data from XMM-Newton and the Sloan Digital Sky
   Survey. Figure 5 is based upon data from with the NASA/ESA Hubble Space
   Telescope and obtained from the Hubble Legacy Archive. This research has
   made use of the NASA/IPAC Extragalactic Database (NED), which is
   operated by JPL, Caltech, under contract with NASA.
NR 137
TC 32
Z9 32
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2014
VL 792
IS 2
AR 117
DI 10.1088/0004-637X/792/2/117
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RF
UT WOS:000341172200035
ER

PT J
AU Kane, SR
   Gelino, DM
AF Kane, Stephen R.
   Gelino, Dawn M.
TI ON THE INCLINATION AND HABITABILITY OF THE HD 10180 SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; planetary systems; stars: individual (HD 10180)
ID MAIN-SEQUENCE STARS; EARTH RADII; MASS; ZONE; DEPENDENCE; PLANETS;
   STELLAR; EXOPLANETS; TRANSITS; EXOMOONS
AB There are numerous multi-planet systems that have now been detected via a variety of techniques. These systems exhibit a range of both planetary properties and orbital configurations. For those systems without detected planetary transits, a significant unknown factor is the orbital inclination. This produces an uncertainty in the mass of the planets and their related properties, such as atmospheric scale height. Here we investigate the HD 10180 system, which was discovered using the radial velocity technique. We provide a new orbital solution for the system which allows for eccentric orbits for all planets. We show how the inclination of the system affects the mass/radius properties of the planets and how the detection of phase signatures may resolve the inclination ambiguity. We finally evaluate the Habitable Zone properties of the system and show that the g planet spends 100% of an eccentric orbit within the Habitable Zone.
C1 [Kane, Stephen R.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA.
   [Gelino, Dawn M.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Kane, SR (reprint author), San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA.
EM skane@sfsu.edu
NR 36
TC 2
Z9 2
U1 1
U2 15
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 2014
VL 792
IS 2
AR 111
DI 10.1088/0004-637X/792/2/111
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RF
UT WOS:000341172200029
ER

PT J
AU Levan, AJ
   Tanvir, NR
   Fruchter, AS
   Hjorth, J
   Pian, E
   Mazzali, P
   Hounsell, RA
   Perley, DA
   Cano, Z
   Graham, J
   Cenko, SB
   Fynbo, JPU
   Kouveliotou, C
   Pe'er, A
   Misra, K
   Wiersema, K
AF Levan, A. J.
   Tanvir, N. R.
   Fruchter, A. S.
   Hjorth, J.
   Pian, E.
   Mazzali, P.
   Hounsell, R. A.
   Perley, D. A.
   Cano, Z.
   Graham, J.
   Cenko, S. B.
   Fynbo, J. P. U.
   Kouveliotou, C.
   Pe'er, A.
   Misra, K.
   Wiersema, K.
TI HUBBLE SPACE TELESCOPE OBSERVATIONS OF THE AFTERGLOW, SUPERNOVA, AND
   HOST GALAXY ASSOCIATED WITH THE EXTREMELY BRIGHT GRB 130427A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; supernovae: general
ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; 25 APRIL 1998; LONG;
   DISCOVERY; SIGNATURES; EVOLUTION; REGIONS; 100316D; SEARCH
AB We present Hubble Space Telescope (HST) observations of the exceptionally bright and luminous Swift gamma-ray burst (GRB), GRB 130427A. At z = 0.34, this burst affords an excellent opportunity to study the supernova (SN) and host galaxy associated with an intrinsically extremely luminous burst (E-iso > 1054 erg): more luminous than any previous GRB with a spectroscopically associated SN. We use the combination of the image quality, UV capability, and invariant point-spread function of HST to provide the best possible separation of the afterglow, host, and SN contributions to the observed light similar to 17 rest-frame days after the burst, utilizing a host subtraction spectrum obtained one year later. Advanced Camera for Surveys grism observations show that the associated SN, SN 2013cq, has an overall spectral shape and luminosity similar to SN 1998bw (with a photospheric velocity, upsilon(ph) similar to 15,000 km s(-1)). The positions of the bluer features are better matched by the higher velocity SN 2010bh (upsilon(ph) similar to 30,000 km s(-1)), but this SN is significantly fainter and fails to reproduce the overall spectral shape, perhaps indicative of velocity structure in the ejecta. We find that the burst originated similar to 4 kpc from the nucleus of a moderately star forming (1M(circle dot) yr(-1)), possibly interacting disk galaxy. The absolute magnitude, physical size, and morphology of this galaxy, as well as the location of the GRB within it, are also strikingly similar to those of GRB 980425/SN 1998bw. The similarity of the SNe and environment from both the most luminous and least luminous GRBs suggests that broadly similar progenitor stars can create GRBs across six orders of magnitude in isotropic energy.
C1 [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
   [Tanvir, N. R.; Wiersema, K.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
   [Fruchter, A. S.; Hounsell, R. A.; Graham, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Hjorth, J.; Fynbo, J. P. U.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
   [Pian, E.] INAF, Trieste Astron Observ, I-34143 Trieste, Italy.
   [Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy.
   [Pian, E.] European So Observ, D-85748 Garching, Germany.
   [Mazzali, P.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England.
   [Perley, D. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
   [Cano, Z.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland.
   [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
   [Kouveliotou, C.] NASA, Marshall Space Flight Ctr, Sci & Technol Off, Huntsville, AL 35812 USA.
   [Pe'er, A.] Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland.
   [Misra, K.] Aryabhatta Res Inst Observat Sci, Naini Tal 263002, India.
RP Levan, AJ (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
EM a.j.levan@warwick.ac.uk
RI Fynbo, Johan/L-8496-2014; Hjorth, Jens/M-5787-2014; 
OI Fynbo, Johan/0000-0002-8149-8298; Hjorth, Jens/0000-0002-4571-2306;
   Pian, Elena/0000-0001-8646-4858
FU STFC; DNRF
FX We thank Matt Mountain and the STScI staff for rapidly scheduling our
   observations. A.J.L. thanks the Leverhulme Trust. A.J.L., N.R.T., and
   K.W. are supported by STFC. The Dark Cosmology Centre is funded by the
   DNRF. 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 Nos. 13230, 13110, and 13117.
NR 47
TC 14
Z9 14
U1 2
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2014
VL 792
IS 2
AR 115
DI 10.1088/0004-637X/792/2/115
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RF
UT WOS:000341172200033
ER

PT J
AU Mawet, D
   Milli, J
   Wahhaj, Z
   Pelat, D
   Absil, O
   Delacroix, C
   Boccaletti, A
   Kasper, M
   Kenworthy, M
   Marois, C
   Mennesson, B
   Pueyo, L
AF Mawet, D.
   Milli, J.
   Wahhaj, Z.
   Pelat, D.
   Absil, O.
   Delacroix, C.
   Boccaletti, A.
   Kasper, M.
   Kenworthy, M.
   Marois, C.
   Mennesson, B.
   Pueyo, L.
TI FUNDAMENTAL LIMITATIONS OF HIGH CONTRAST IMAGING SET BY SMALL SAMPLE
   STATISTICS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: statistical; techniques: high angular resolution
ID PHASE-MASK CORONAGRAPH; DYNAMIC-RANGE; PLANET DETECTION; PINNED
   SPECKLES; HD 95086; COMPANIONS; IMAGES; LIMITS; BEAMWIDTHS; PRINCIPLE
AB In this paper, we review the impact of small sample statistics on detection thresholds and corresponding confidence levels (CLs) in high-contrast imaging at small angles. When looking close to the star, the number of resolution elements decreases rapidly toward small angles. This reduction of the number of degrees of freedom dramatically affects CLs and false alarm probabilities. Naively using the same ideal hypothesis and methods as for larger separations, which are well understood and commonly assume Gaussian noise, can yield up to one order of magnitude error in contrast estimations at fixed CL. The statistical penalty exponentially increases toward very small inner working angles. Even at 5-10 resolution elements from the star, false alarm probabilities can be significantly higher than expected. Here we present a rigorous statistical analysis that ensures robustness of the CL, but also imposes a substantial limitation on corresponding achievable detection limits (thus contrast) at small angles. This unavoidable fundamental statistical effect has a significant impact on current coronagraphic and future high-contrast imagers. Finally, the paper concludes with practical recommendations to account for small number statistics when computing the sensitivity to companions at small angles and when exploiting the results of direct imaging planet surveys.
C1 [Mawet, D.; Milli, J.; Wahhaj, Z.] European So Observ, Santiago, Chile.
   [Pelat, D.] UPMC, CNRS, Observ Paris, LUTH, F-92195 Meudon, France.
   [Pelat, D.; Boccaletti, A.] Univ Paris Diderot, F-92195 Meudon, France.
   [Absil, O.; Delacroix, C.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Cointe Ougree, Belgium.
   [Boccaletti, A.] UPMC, CNRS, Observ Paris, LESIA, F-92195 Meudon, France.
   [Kasper, M.] European Southern Observ Headquarters, D-85748 Garching, Germany.
   [Kenworthy, M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
   [Marois, C.] Herzberg Inst Astrophys, NRC, Victoria, BC V9E 2E7, Canada.
   [Mennesson, B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Pueyo, L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Mawet, D (reprint author), European So Observ, Alonso Cordova 3107, Santiago, Chile.
OI Absil, Olivier/0000-0002-4006-6237; Delacroix,
   Christian/0000-0003-0150-4430
FU European Research Council [337569]; French Community of Belgium through
   an ARC
FX This work was carried out at the European Southern Observatory (ESO)
   site of Vitacura (Santiago, Chile). The authors thank the referee,
   Professor Dmitry Savransky, for his critical, thorough, and very
   constructive review of the manuscript. The research leading to these
   results has received funding from the European Research Council Under
   the European Union's Seventh Framework Programme (ERC Grant Agreement n.
   337569) and from the French Community of Belgium through an ARC grant
   for Concerted Research Action. 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 55
TC 36
Z9 36
U1 1
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2014
VL 792
IS 2
AR 97
DI 10.1088/0004-637X/792/2/97
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RF
UT WOS:000341172200015
ER

PT J
AU Puzzarini, C
   Ali, A
   Biczysko, M
   Barone, V
AF Puzzarini, Cristina
   Ali, Ashraf
   Biczysko, Malgorzata
   Barone, Vincenzo
TI ACCURATE SPECTROSCOPIC CHARACTERIZATION OF PROTONATED OXIRANE: A
   POTENTIAL PREBIOTIC SPECIES IN TITAN'S ATMOSPHERE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: molecules; line: identification; methods: data analysis; molecular
   data
ID CORRELATED MOLECULAR CALCULATIONS; ANHARMONIC VIBRATIONAL PROPERTIES;
   ABSOLUTE LINE-INTENSITIES; GAUSSIAN-BASIS SETS; ETHYLENE-OXIDE; SYSTEMS;
   COMPUTATIONS; AFFINITIES; BANDS; BORON
AB An accurate spectroscopic characterization of protonated oxirane has been carried out by means of state-of-the-art computational methods and approaches. The calculated spectroscopic parameters from our recent computational investigation of oxirane together with the corresponding experimental data available were used to assess the accuracy of our predicted rotational and IR spectra of protonated oxirane. We found an accuracy of about 10 cm(-1) for vibrational transitions (fundamentals as well as overtones and combination bands) and, in relative terms, of 0.1% for rotational transitions. We are therefore confident that the spectroscopic data provided herein are a valuable support for the detection of protonated oxirane not only in Titan's atmosphere but also in the interstellar medium.
C1 [Puzzarini, Cristina] Univ Bologna, Dipartimento Chim Giacomo Ciamician, I-40126 Bologna, Italy.
   [Ali, Ashraf] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Biczysko, Malgorzata; Barone, Vincenzo] Scuola Normale Super Pisa, I-56126 Pisa, Italy.
   [Biczysko, Malgorzata] UOS Pisa, Area Ric CNR, Ist Chim Composti OrganoMet ICCOM CNR, I-56124 Pisa, Italy.
RP Puzzarini, C (reprint author), Univ Bologna, Dipartimento Chim Giacomo Ciamician, Via Selmi 2, I-40126 Bologna, Italy.
EM cristina.puzzarini@unibo.it
RI Barone, Vincenzo/C-7344-2008; Biczysko, Malgorzata/D-1300-2009;
   PUZZARINI, CRISTINA/E-4640-2015
OI Biczysko, Malgorzata/0000-0002-6439-5561; PUZZARINI,
   CRISTINA/0000-0002-2395-8532
FU Italian MIUR (PRIN "STAR: Spectroscopic and computational Techniques for
   Astrophysical and atmospheric Research") [PON01-01078/8]; University of
   Bologna (RFO funds); NASA Goddard Space Flight Center by the Cassini
   Plasma Spectrometer (CAPS) Project through NASA Jet Propulsion
   Laboratory [1243218]; Southwest Research Institute in San Antonio, TX;
   COST CMTS-Action [CM1002]; European Union [ERC-2012-AdG-320951-DREAMS]
FX This work was supported by the Italian MIUR (PRIN 2012 "STAR:
   Spectroscopic and computational Techniques for Astrophysical and
   atmospheric Research" and PON01-01078/8) and by the University of
   Bologna (RFO funds). This work was also supported in part at the NASA
   Goddard Space Flight Center by the Cassini Plasma Spectrometer (CAPS)
   Project through NASA Jet Propulsion Laboratory contract 1243218 with the
   Southwest Research Institute in San Antonio, TX. The high performance
   computer facilities of the DREAMS center (http://dreamshpc.sns.it) are
   acknowledged for providing computer resources. The support of COST
   CMTS-Action CM1002 "COnvergent Distributed Environment for Computational
   Spectroscopy (CODECS)" is also acknowledged. The research leading to
   these results has received funding from the European Union's Seventh
   Framework Programme (FP7/2007-2013) under grant agreement No
   ERC-2012-AdG-320951-DREAMS.
NR 38
TC 5
Z9 5
U1 1
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2014
VL 792
IS 2
AR 118
DI 10.1088/0004-637X/792/2/118
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RF
UT WOS:000341172200036
ER

PT J
AU Upton, L
   Hathaway, DH
AF Upton, Lisa
   Hathaway, David H.
TI EFFECTS OF MERIDIONAL FLOW VARIATIONS ON SOLAR CYCLES 23 AND 24
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: magnetic fields; sunspots
ID POLAR MAGNETIC-FIELDS; FLUX-TRANSPORT; SUNSPOT CYCLE-21; SURFACE; SUN;
   EVOLUTION; SIMULATIONS; DYNAMICS; STRENGTH; IMAGER
AB The faster meridional flow that preceded the solar cycle 23/24 minimum is thought to have led to weaker polar field strengths, producing the extended solar minimum and the unusually weak cycle 24. To determine the impact of meridional flow variations on the sunspot cycle, we have simulated the Sun's surface magnetic field evolution with our newly developed surface flux transport model. We investigate three different cases: a constant average meridional flow, the observed time-varying meridional flow, and a time-varying meridional flow in which the observed variations from the average have been doubled. Comparison of these simulations shows that the variations in the meridional flow over cycle 23 have a significant impact (similar to 20%) on the polar fields. However, the variations produced polar fields that were stronger than they would have been otherwise. We propose that the primary cause of the extended cycle 23/24 minimum and weak cycle 24 was the weakness of cycle 23 itself-with fewer sunspots, there was insufficient flux to build a big cycle. We also find that any polar counter-cells in the meridional flow (equatorward flow at high latitudes) produce flux concentrations at mid-to-high latitudes that are not consistent with observations.
C1 [Upton, Lisa] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
   [Upton, Lisa] Univ Alabama, Ctr Space Phys & Aeron Res, Huntsville, AL 35899 USA.
   [Hathaway, David H.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Upton, L (reprint author), Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
EM lisa.a.upton@vanderbilt.edu; david.hathaway@nasa.gov
FU NASA [NAG5-10483]
FX The authors were supported by a grant from the NASA Living with a Star
   Program to Marshall Space Flight Center. The HMI data used are courtesy
   of the NASA/SDO and the HMI science team. The SOHO/MDI project was
   supported by NASA grant NAG5-10483 to Stanford University. SOHO is a
   project of international cooperation between ESA and NASA.
NR 35
TC 4
Z9 4
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2014
VL 792
IS 2
AR 142
DI 10.1088/0004-637X/792/2/142
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AO2RF
UT WOS:000341172200060
ER

PT J
AU Xie, YS
   Fan, X
   Wilson, JD
   Simons, RN
   Chen, YP
   Xiao, JQ
AF Xie, Yunsong
   Fan, Xin
   Wilson, Jeffrey D.
   Simons, Rainee N.
   Chen, Yunpeng
   Xiao, John Q.
TI A universal electromagnetic energy conversion adapter based on a
   metamaterial absorber
SO SCIENTIFIC REPORTS
LA English
DT Article
ID SOLAR-CELLS; BAND; TRANSMISSION; PLASMONICS; ANTENNAS; RECTENNA
AB On the heels of metamaterial absorbers (MAs) which produce near perfect electromagnetic (EM) absorption and emission, we propose a universal electromagnetic energy conversion adapter (UEECA) based on MA. By choosing the appropriate energy converting sensors, the UEECA is able to achieve near 100% signal transfer ratio between EM energy and various forms of energy such as thermal, DC electric, or higher harmonic EM energy. The inherited subwavelength dimension and the EM field intensity enhancement can further empower UEECA in many critical applications such as energy harvesting, photoconductive antennas, and nonlinear optics. The principle of UEECA is understood with a transmission line model, which further provides a design strategy that can incorporate a variety of energy conversion devices. The concept is experimentally validated at a microwave frequency with a signal transfer ratio of 96% by choosing an RF diode as the energy converting sensor.
C1 [Xie, Yunsong; Fan, Xin; Chen, Yunpeng; Xiao, John Q.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
   [Wilson, Jeffrey D.; Simons, Rainee N.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Xiao, JQ (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
EM jqx@udel.edu
RI Chen, Yunpeng/C-9764-2017
OI Chen, Yunpeng/0000-0002-9785-4111
FU NASA EPSCoR program [NNX11AQ29A]
FX The authors thank the discussions with Dr. Qi Lu. The work is supported
   from the NASA EPSCoR program under grant number NNX11AQ29A.
NR 29
TC 4
Z9 4
U1 6
U2 79
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 9
PY 2014
VL 4
AR 6301
DI 10.1038/srep06301
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AP2UX
UT WOS:000341932300005
PM 25200005
ER

PT J
AU Berleman, JE
   Allen, S
   Danielewicz, MA
   Remis, JP
   Gorur, A
   Cunha, J
   Hadi, MZ
   Zusman, DR
   Northen, TR
   Witkowska, HE
   Auer, M
AF Berleman, James E.
   Allen, Simon
   Danielewicz, Megan A.
   Remis, Jonathan P.
   Gorur, Amita
   Cunha, Jack
   Hadi, Masood Z.
   Zusman, David R.
   Northen, Trent R.
   Witkowska, H. Ewa
   Auer, Manfred
TI The lethal cargo of Myxococcus xanthus outer membrane vesicles
SO FRONTIERS IN MICROBIOLOGY
LA English
DT Article
DE predation; fruiting body; predatory rippling; predator-prey
   interactions; secondary metabolism and enzymes
ID MASS-SPECTROMETRY; ESCHERICHIA-COLI; PROTEOMICS; PROTEIN; MYXOBACTERIA;
   BACTERIA; REPRODUCIBILITY; BIOSYNTHESIS; ENVIRONMENTS; MYXOVIRESCIN
AB Myxococcus xanthus is a bacterial micro-predator known for hunting other microbes in a wolf pack-like manner. Outer membrane vesicles (OMVs) are produced in large quantities by M. xanthus and have a highly organized structure in the extracellular milieu, sometimes occurring in chains that link neighboring cells within a biofilm. OMVs may be a vehicle for mediating wolf pack activity by delivering hydrolytic enzymes and antibiotics aimed at killing prey microbes. Here, both the protein and small molecule cargo of the OMV and membrane fractions of M. xanthus were characterized and compared. Our analysis indicates a number of proteins that are OMV-specific or OMV-enriched, including several with putative hydrolytic function. Secondary metabolite profiling of OMVs identifies 16 molecules, many associated with antibiotic activities. Several hydrolytic enzyme homologs were identified, including the protein encoded by MXAN_3564 (mepA), an M36 protease homolog. Genetic disruption of mepA leads to a significant reduction in extracellular protease activity suggesting MepA is part of the long-predicted (yet to date undetermined) extracellular protease suite of M. xanthus.
C1 [Berleman, James E.; Danielewicz, Megan A.; Remis, Jonathan P.; Gorur, Amita; Cunha, Jack; Hadi, Masood Z.; Northen, Trent R.; Auer, Manfred] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Life Sci, Berkeley, CA 94720 USA.
   [Berleman, James E.; Zusman, David R.] Univ Calif Berkeley, Dept Cell & Mol Biol, Berkeley, CA 94720 USA.
   [Berleman, James E.] St Marys Coll, Sch Biol, Moraga, CA 94575 USA.
   [Allen, Simon; Witkowska, H. Ewa] Univ Calif San Francisco, Dept Obstet Gynecol & Reprod Sci, Sandler Moore Mass Spectrometry Core Facil, San Francisco, CA USA.
   [Hadi, Masood Z.] NASA, Ames Res Ctr, Space Biosci Div, Synthet Biol Program, Moffett Field, CA 94035 USA.
   [Hadi, Masood Z.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Phys Biosci Div, Berkeley, CA 94720 USA.
RP Auer, M (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Life Sci, Berkeley, CA 94720 USA.
EM mauer@lbl.gov
OI Northen, Trent/0000-0001-8404-3259
FU National Institutes of Health [5R01GMO20509, 3R01GMO20509-3651]; Office
   of Biological and Environmental Research of the US Department of Energy
   [DE-ACO2-05CH11231]; US Department of Energy VFP program; Sandler Family
   Foundation; Gordon and Betty Moore Foundation; NIH/NCI Cancer Center
   Support Grant [P30 CA082103]
FX We thank Dr. Emilia Mauriello, for her advice and discussion and Marcin
   Zemla for technical assistance. We would also like to thank the Auer Lab
   for helpful discussions. This work was supported by the National
   Institutes of Health (5R01GMO20509 and 3R01GMO20509-3651 to David R.
   Zusman), by Lab directed research development funds from the Office of
   Biological and Environmental Research of the US Department of Energy
   under contract number DE-ACO2-05CH11231 (to Manfred Auer and Trent R.
   Northen) and the US Department of Energy VFP program (James E.
   Berleman). Mass spectrometry analysis was performed by the UCSF
   Sandler-Moore Mass Spectrometry Core Facility, which acknowledges
   support from the Sandler Family Foundation, the Gordon and Betty Moore
   Foundation, and NIH/NCI Cancer Center Support Grant P30 CA082103.
NR 55
TC 16
Z9 16
U1 1
U2 25
PU FRONTIERS RESEARCH FOUNDATION
PI LAUSANNE
PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND
SN 1664-302X
J9 FRONT MICROBIOL
JI Front. Microbiol.
PD SEP 9
PY 2014
VL 5
AR 474
DI 10.3389/fmicb.2014.00474
PG 11
WC Microbiology
SC Microbiology
GA AO9PQ
UT WOS:000341688200001
PM 25250022
ER

PT J
AU Yoon, JS
   Rim, T
   Kim, J
   Meyyappan, M
   Baek, CK
   Jeong, YH
AF Yoon, Jun-Sik
   Rim, Taiuk
   Kim, Jungsik
   Meyyappan, Meyya
   Baek, Chang-Ki
   Jeong, Yoon-Ha
TI Vertical gate-all-around junctionless nanowire transistors with
   asymmetric diameters and underlap lengths
SO APPLIED PHYSICS LETTERS
LA English
DT Article
AB Vertical gate-all-around (GAA) junctionless nanowire transistors (JNTs) with different diameters and underlap lengths are investigated using three-dimensional device simulations. The source-side diameter determines the on-current and drain-induced barrier lowering characteristics, whereas the drain-side diameter controls the band-to-band tunneling current during off-state conditions. The JNTs with short drain-side underlap lengths decrease the source/drain series resistance but increase the off-current values, especially due to large band-gap narrowing effects at the drain extension region. Proper device design of vertical GAA JNTs considering the device structure and underlap is needed to improve both on/off and short channel characteristics. (C) 2014 AIP Publishing LLC.
C1 [Yoon, Jun-Sik; Rim, Taiuk; Baek, Chang-Ki] Pohang Univ Sci & Technol, Dept Creat IT Engn, Pohang 790784, South Korea.
   [Yoon, Jun-Sik; Rim, Taiuk; Baek, Chang-Ki] Pohang Univ Sci & Technol, Future IT Innovat Lab, Pohang 790784, South Korea.
   [Kim, Jungsik; Meyyappan, Meyya] Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang 790784, South Korea.
   [Meyyappan, Meyya] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Baek, Chang-Ki; Jeong, Yoon-Ha] Pohang Univ Sci & Technol, Dept Elect Engn, Pohang 790784, South Korea.
RP Yoon, JS (reprint author), Pohang Univ Sci & Technol, Dept Creat IT Engn, Pohang 790784, South Korea.
FU MSIP (Ministry of Science, ICT and Future Planning), Korea under "IT
   Consilience Creative Program" [NIPA-2014-H0201-14-1001]; IDEC (IC Design
   Education Center)
FX This research was supported by the MSIP (Ministry of Science, ICT and
   Future Planning), Korea, under the "IT Consilience Creative Program"
   (NIPA-2014-H0201-14-1001) supervised by the NIPA (National IT Industry
   Promotion Agency) and also supported by IDEC (IC Design Education
   Center).
NR 17
TC 3
Z9 3
U1 4
U2 26
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
   MELVILLE, NY 11747-4501 USA
SN 0003-6951
EI 1077-3118
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD SEP 8
PY 2014
VL 105
IS 10
AR 102105
DI 10.1063/1.4895030
PG 4
WC Physics, Applied
SC Physics
GA AQ4IQ
UT WOS:000342758700030
ER

PT J
AU Atli, KC
   Karaman, I
   Noebe, RD
AF Atli, K. C.
   Karaman, I.
   Noebe, R. D.
TI Influence of tantalum additions on the microstructure and shape memory
   response of Ti50.5Ni24.5Pd25 high-temperature shape memory alloy
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
   MICROSTRUCTURE AND PROCESSING
LA English
DT Article
DE High temperature shape memory alloys; TiNiPd; Dimensional stability;
   Martensitic transformation; Shape memory response
ID SEVERE PLASTIC-DEFORMATION; NITIHFPD SINGLE-CRYSTALS; MARTENSITIC
   TRANSFORMATIONS; FUNCTIONAL STABILITY; HYSTERESIS; PRECIPITATION;
   COMPRESSION; PHASE; PD
AB A Ti50.5Ni24.5Pd25 (at%) high-temperature shape memory alloy (HTSMA) was alloyed with 1, 3, and 5 at% Ta additions in an effort to enhance the shape memory properties, particularly the dimensional stability for actuator applications. Thermomechanical characterization indicated that the dimensional stability of Ti50.5Ni24.5Pd25 improved significantly, but mostly for the highest Ta addition. This improvement was attributed in part to a particulate strengthening effect, since both Ti47.5Ni24.5Pd25Ta3 and Ti45.5Ni24.5 Pd25Ta5 were found to have similar amounts of Ta, approximately 2.2 at%, in solid solution. However, by 5% Ta addition, the transformation temperatures decreased by about 65 degrees C and reductions in transformation strain and fracture resistance occurred. Consequently, among the alloys studied, Ti47.5Ni24.5 Pd25Ta3 seemed to be the optimum composition with a transformation temperature around 150 degrees C, a transformation strain value close to that of the unalloyed composition, and improved dimensional stability. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Atli, K. C.] Anadolu Univ, Dept Mech Engn, Eskisehir, Turkey.
   [Karaman, I.] Texas A&M Univ, Dept Mat Sci & Engn, College Stn, TX 77843 USA.
   [Noebe, R. D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
RP Atli, KC (reprint author), Anadolu Univ, Dept Mech Engn, Eskisehir, Turkey.
EM kcatli@anadolu.edu.tr
RI Karaman, Ibrahim/E-7450-2010; Atli, Kadri/D-6978-2013
OI Karaman, Ibrahim/0000-0001-6461-4958; Atli, Kadri/0000-0002-4807-2113
FU NASA Fundamental Aeronautics Program, Subsonic Fixed Wing project
   [NNX07AB56A]; FAP Aeronautical Sciences Project; US Air Force Office of
   Scientific Research [FA9550-12-1-0218]
FX This study has been supported by the NASA Fundamental Aeronautics
   Program, Subsonic Fixed Wing project through Cooperative Agreement no.
   NNX07AB56A, with additional support from the FAP Aeronautical Sciences
   Project. IK acknowledges the support from the US Air Force Office of
   Scientific Research, Grant no. FA9550-12-1-0218. The authors wish to
   thank Dr. Ray Guillemette of Texas A&M University Geology & Geophysics
   Department for the microprobe analyses and the Shape Memory Alloy Group
   at NASA Glenn Research Center for helpful discussions.
NR 40
TC 7
Z9 7
U1 3
U2 23
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0921-5093
EI 1873-4936
J9 MAT SCI ENG A-STRUCT
JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process.
PD SEP 8
PY 2014
VL 613
BP 250
EP 258
DI 10.1016/j.msea.2014.06.104
PG 9
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
   Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
   Metallurgical Engineering
GA AO4UM
UT WOS:000341336900030
ER

PT J
AU Chopovsky, A
   Eingorn, M
   Zhuk, A
AF Chopovsky, Alexey
   Eingorn, Maxim
   Zhuk, Alexander
TI Problematic aspects of Kaluza-Klein excitations in multidimensional
   models with Einstein internal spaces
SO PHYSICS LETTERS B
LA English
DT Article
DE Multidimensional models; Kaluza-Klein models; Kaluza-Klein
   excitations/modes; Einstein spaces; Black strings/branes; Gravitational
   tests
ID DIMENSIONAL REDUCTION; MASS-SPECTRUM; SUPERGRAVITY
AB We consider Kaluza-Klein (KK) models where internal spaces are compact Einstein spaces. These spaces are stabilized by background matter (e.g., monopole form-fields). We perturb this background by a compact matter source (e.g., the system of gravitating masses) with the zero pressure in the external/our space and an arbitrary pressure in the internal space. We show that the Einstein equations are compatible only if the matter source is smeared over the internal space and perturbed metric components do not depend on coordinates of extra dimensions. The latter means the absence of KK modes corresponding to the metric fluctuations. Maybe, the absence of KK particles in LHC experiments is explained by such mechanism. (C) 2014 The Authors. Published by Elsevier B.V.
C1 [Chopovsky, Alexey] Odessa Natl Univ, Dept Theoret Phys, UA-65082 Odessa, Ukraine.
   [Chopovsky, Alexey; Zhuk, Alexander] Odessa Natl Univ, Astron Observ, UA-65082 Odessa, Ukraine.
   [Eingorn, Maxim] N Carolina Cent Univ, CREST, Durham, NC 27707 USA.
   [Eingorn, Maxim] N Carolina Cent Univ, NASA, Res Ctr, Durham, NC 27707 USA.
RP Zhuk, A (reprint author), Odessa Natl Univ, Astron Observ, Dvoryanskaya St 2, UA-65082 Odessa, Ukraine.
EM a.chopovsky@yandex.ru; maxim.eingorn@gmail.com; ai.zhuk2@gmail.com
RI Eingorn, Maxim/L-1543-2014; 
OI Eingorn, Maxim/0000-0002-1545-7818; Zhuk, Alexander/0000-0001-9107-5048;
   Chopovsky, Alexey/0000-0002-2405-5669
FU NSF CREST [HRD-1345219]; NASA [NNX09AV07A]
FX The work of M. Eingorn was supported by NSF CREST award HRD-1345219 and
   NASA grant NNX09AV07A. A. Zhuk acknowledges the hospitality of the
   Theory Division of CERN during the final preparation of this paper.
NR 27
TC 1
Z9 1
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0370-2693
EI 1873-2445
J9 PHYS LETT B
JI Phys. Lett. B
PD SEP 7
PY 2014
VL 736
BP 329
EP 332
DI 10.1016/j.physletb.2014.07.042
PG 4
WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA AO6UR
UT WOS:000341487800049
ER

PT J
AU Caluwaerts, K
   Despraz, J
   Iscen, A
   Sabelhaus, AP
   Bruce, J
   Schrauwen, B
   SunSpiral, V
AF Caluwaerts, Ken
   Despraz, Jeremie
   Iscen, Atil
   Sabelhaus, Andrew P.
   Bruce, Jonathan
   Schrauwen, Benjamin
   SunSpiral, Vytas
TI Design and control of compliant tensegrity robots through simulation and
   hardware validation
SO JOURNAL OF THE ROYAL SOCIETY INTERFACE
LA English
DT Article
DE tensegrity; bioinspired locomotion; central pattern generators;
   compliant robotics; soft robotics; planetary exploration
ID DYNAMIC-ANALYSIS; LOCOMOTION; MODEL; COMMUNICATION; GENERATORS;
   FRAMEWORKS; RULES
AB To better understand the role of tensegrity structures in biological systems and their application to robotics, the Dynamic Tensegrity Robotics Lab at NASA Ames Research Center, Moffett Field, CA, USA, has developed and validated two software environments for the analysis, simulation and design of tensegrity robots. These tools, along with newcontrol methodologies and the modular hardware components developed to validate them, are presented as a system for the design of actuated tensegrity structures. As evidenced from their appearance in many biological systems, tensegrity ('tensile-integrity') structures have unique physical properties that make them ideal for interaction with uncertain environments. Yet, these characteristics make design and control of bioinspired tensegrity robots extremely challenging. This work presents the progress our tools have made in tackling the design and control challenges of spherical tensegrity structures. We focus on this shape since it lends itself to rolling locomotion. The results of our analyses include multiple novel control approaches for mobility and terrain interaction of spherical tensegrity structures that have been tested in simulation. A hardware prototype of a spherical six-bar tensegrity, the Reservoir Compliant Tensegrity Robot, is used to empirically validate the accuracy of simulation.
C1 [Caluwaerts, Ken; Despraz, Jeremie; Iscen, Atil; Sabelhaus, Andrew P.; Bruce, Jonathan; SunSpiral, Vytas] NASA, Ames Res Ctr, Dynam Tensegr Robot Lab, Moffett Field, CA 94035 USA.
   [Caluwaerts, Ken; Schrauwen, Benjamin] Univ Ghent, Dept Elect & Informat Syst, Reservoir Lab, B-9000 Ghent, Belgium.
   [Despraz, Jeremie] Ecole Polytech Fed Lausanne, Biorobot Lab, CH-1015 Lausanne, Switzerland.
   [Iscen, Atil] Oregon State Univ, Sch Elect Engn & Comp Sci, Corvallis, OR 97331 USA.
   [Sabelhaus, Andrew P.] Univ Calif Berkeley, Berkeley Inst Design, Berkeley, CA 94720 USA.
   [Bruce, Jonathan] Univ Calif Santa Cruz, USRA, Santa Cruz, CA 95064 USA.
   [SunSpiral, Vytas] NASA, SGT Inc, Ames Intelligent Robot Grp, Moffett Field, CA USA.
RP Caluwaerts, K (reprint author), NASA, Ames Res Ctr, Dynam Tensegr Robot Lab, Moffett Field, CA 94035 USA.
EM ken.caluwaerts@ugent.be
FU European Commission [248311-AMARSi]; NASA; Research Foundation-Flanders
   (FWO); NSF [DGE1106400]; NASA [NAS2-03144]
FX This research was supported by the European Commission's FP7 programme
   under grant agreement no. 248311-AMARSi and the NASA Innovative Advanced
   Concepts program. K. C. was supported by a PhD fellowship of the
   Research Foundation-Flanders (FWO). Support also came from NSF Graduate
   Research Fellowship no. DGE1106400, and from NASA Prime Contract no.
   NAS2-03144 awarded to the University of California, Santa Cruz,
   University Affiliated Research Center.
NR 48
TC 20
Z9 20
U1 2
U2 19
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1742-5689
EI 1742-5662
J9 J R SOC INTERFACE
JI J. R. Soc. Interface
PD SEP 6
PY 2014
VL 11
IS 98
AR 20140520
DI 10.1098/rsif.2014.0520
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AK6DW
UT WOS:000338519300015
PM 24990292
ER

PT J
AU Ducluzeau, AL
   Schoepp-Cothenet, B
   van Lis, R
   Baymann, F
   Russell, MJ
   Nitschke, W
AF Ducluzeau, Anne-Lise
   Schoepp-Cothenet, Barbara
   van Lis, Robert
   Baymann, Frauke
   Russell, Michael J.
   Nitschke, Wolfgang
TI The evolution of respiratory O-2/NO reductases: an
   out-of-the-phylogenetic-box perspective
SO JOURNAL OF THE ROYAL SOCIETY INTERFACE
LA English
DT Review
DE O-2-reductase; NO-reductase; haem-copper oxidase; origin and evolution
   of respiration; palaeogeochemistry
ID NITRIC-OXIDE REDUCTASE; COPPER OXYGEN REDUCTASES; FACULTATIVELY
   ANAEROBIC-BACTERIA; ELECTRON-PARAMAGNETIC-RESONANCE; BILLION YEARS AGO;
   ESCHERICHIA-COLI; THERMUS-THERMOPHILUS; AEROBIC METABOLISM; NITRATE
   REDUCTASE; GEOBACILLUS-STEAROTHERMOPHILUS
AB Complex life on our planet crucially depends on strong redox disequilibria afforded by the almost ubiquitous presence of highly oxidizing molecular oxygen. However, the history of O-2-levels in the atmosphere is complex and prior to the Great Oxidation Event some 2.3 billion years ago, the amount of O-2 in the biosphere is considered to have been extremely low as compared with present-day values. Therefore the evolutionary histories of life and of O-2-levels are likely intricately intertwined. The obvious biological proxy for inferring the impact of changing O-2-levels on life is the evolutionary history of the enzyme allowing organisms to tap into the redox power of molecular oxygen, i. e. the bioenergetic O-2 reductases, alias the cytochrome and quinol oxidases. Consequently, molecular phylogenies reconstructed for this enzyme superfamily have been exploited over the last two decades in attempts to elucidate the interlocking between O-2 levels in the environment and the evolution of respiratory bioenergetic processes. Although based on strictly identical datasets, these phylogenetic approaches have led to diametrically opposite scenarios with respect to the history of both the enzyme superfamily and molecular oxygen on the Earth. In an effort to overcome the deadlock of molecular phylogeny, we here review presently available structural, functional, palaeogeochemical and thermodynamic information pertinent to the evolution of the superfamily (which notably also encompasses the subfamily of nitric oxide reductases). The scenario which, in our eyes, most closely fits the ensemble of these non-phylogenetic data, sees the low O-2-affinity SoxM- (orA-) type enzymes as the most recent evolutionary innovation and the high-affinity O-2 reductases (SoxB or B and cbb(3) or C) as arising independently from NO-reducing precursor enzymes.
C1 [Schoepp-Cothenet, Barbara; van Lis, Robert; Baymann, Frauke; Nitschke, Wolfgang] Univ Aix Marseille, CNRS, UMR 7281, Lab Bioenerget & Ingn Prot,FR3479, F-13402 Marseille 20, France.
   [Russell, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Ducluzeau, Anne-Lise] Univ Nebraska, Beadle Ctr, Lincoln, NE 68588 USA.
RP Nitschke, W (reprint author), Univ Aix Marseille, CNRS, UMR 7281, Lab Bioenerget & Ingn Prot,FR3479, F-13402 Marseille 20, France.
EM nitschke@imm.cnrs.fr
OI Nitschke, Wolfgang/0000-0003-2084-3032
FU National Aeronautics and Space Administration; NASA Exobiology and
   Evolutionary Biology award [NNH06ZDA001N]; NASA Astrobiology Institute
   (Icy Worlds); ANR [06-BLAN-0384]
FX M.J.R.'s contribution 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 NASA Exobiology
   and Evolutionary Biology award (NNH06ZDA001N) and supported by the NASA
   Astrobiology Institute (Icy Worlds). Part of the results described in
   this article were obtained by A. L. D., W.N. and R.vL. while supported
   by the ANR grant no. 06-BLAN-0384.
NR 118
TC 8
Z9 8
U1 2
U2 32
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1742-5689
EI 1742-5662
J9 J R SOC INTERFACE
JI J. R. Soc. Interface
PD SEP 6
PY 2014
VL 11
IS 98
AR 20140196
DI 10.1098/rsif.2014.0196
PG 22
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AK6DW
UT WOS:000338519300002
PM 24968694
ER

PT J
AU Pasham, DR
   Strohmayer, TE
   Mushotzky, RF
AF Pasham, Dheeraj R.
   Strohmayer, Tod E.
   Mushotzky, Richard F.
TI A 400-solar-mass black hole in the galaxy M82
SO NATURE
LA English
DT Article
ID QUASI-PERIODIC OSCILLATIONS; X-RAY SOURCE; MICROQUASAR GRO J1655-40; XTE
   J1550-564; RXTE OBSERVATIONS; TIMING EXPLORER; DOMINANT STATE; MASS;
   X-1; DISCOVERY
AB M82 X-1, the brightest X-ray source in the galaxy M82, has been thought to be an intermediate-mass black hole (100 to 10,000 solar masses) because of its extremely high luminosity and variability characteristics(1-6), although some models suggest that its mass may be only about 20 solar masses(3,7). The previous mass estimates were based on scaling relations that use low-frequency characteristic time-scales which have large intrinsic uncertainties(8,9). For stellar-mass black holes, we know that the high-frequency quasi-periodic oscillations (100-450 hertz) in the X-ray emission that occur in a 3: 2 frequency ratio are stable and scale in frequency inversely with black hole mass with a reasonably small dispersion(10-15). The discovery of such stable oscillations thus potentially offers an alternative and less ambiguous means of mass determination for intermediate-mass black holes, but has hitherto not been realized. Here we report stable, twin-peak (3: 2 frequency ratio) X-ray quasi-periodic oscillations from M82 X-1 at frequencies of 3.32+/-0.06 hertz and 5.07+/-0.06 hertz. Assuming that we can extrapolate the inverse-mass scaling that holds for stellar-mass black holes, we estimate the black hole mass of M82 X-1 to be 428+/-105 solar masses. In addition, we can estimate the mass using the relativistic precession model, from which we get a value of 415+/-63 solar masses.
C1 [Pasham, Dheeraj R.; Mushotzky, Richard F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Pasham, Dheeraj R.; Strohmayer, Tod E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
   [Pasham, Dheeraj R.; Strohmayer, Tod E.] NASA, Goddard Space Flight Ctr, Joint Space Sci Inst, Greenbelt, MD 20771 USA.
RP Pasham, DR (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM dheeraj@astro.umd.edu
NR 48
TC 59
Z9 59
U1 1
U2 5
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 4
PY 2014
VL 513
IS 7516
BP 74
EP +
DI 10.1038/nature13710
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AO2SD
UT WOS:000341174800032
PM 25132552
ER

PT J
AU Pickell, PD
   Hermosilla, T
   Coops, NC
   Masek, JG
   Franks, S
   Huang, CQ
AF Pickell, Paul D.
   Hermosilla, Txomin
   Coops, Nicholas C.
   Masek, Jeffrey G.
   Franks, Shannon
   Huang, Chengquang
TI Monitoring anthropogenic disturbance trends in an industrialized boreal
   forest with Landsat time series
SO REMOTE SENSING LETTERS
LA English
DT Article
ID PATTERNS; CLASSIFICATION
AB Human transformation of the terrestrial biosphere via resource utilization is a critical impetus for monitoring and characterizing anthropogenic change to vegetation condition. The primary objective of this research was to detect anthropogenic forest disturbance for a recent Landsat time series. A novel combination of an autonomous change detection procedure and spectral classification scheme was applied and tested in a landscape that has undergone significant resource development over the last 30years. Anthropogenic disturbance was detected with greater than 93% accuracy. Most disturbances were correctly classified as within +/- 1year. The signal of anthropogenic disturbance was significant in the landscape, accounting for more than 91% of all disturbances and 86% of total disturbed area during the 23-year study period. The study demonstrated a robust approach for examining historical disturbance trends related to human-modification of the environment.
C1 [Pickell, Paul D.; Hermosilla, Txomin; Coops, Nicholas C.] Univ British Columbia, Dept Forest Resources Management, Vancouver, BC V5Z 1M9, Canada.
   [Masek, Jeffrey G.] NASA Goddard Space Flight Ctr, Biospher Sci Lab Code 618, Greenbelt, MD USA.
   [Franks, Shannon] SGT Inc, Greenbelt, MD USA.
   [Huang, Chengquang] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
RP Pickell, PD (reprint author), Univ British Columbia, Dept Forest Resources Management, Vancouver, BC V5Z 1M9, Canada.
EM paul.pickell@forestry.ubc.ca
RI Masek, Jeffrey/D-7673-2012; Coops, Nicholas/J-1543-2012; Hermosilla,
   Txomin/K-6206-2014; 
OI Coops, Nicholas/0000-0002-0151-9037; Hermosilla,
   Txomin/0000-0002-5445-0360; Pickell, Paul/0000-0003-4969-0279
NR 36
TC 11
Z9 11
U1 0
U2 17
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 2150-704X
EI 2150-7058
J9 REMOTE SENS LETT
JI Remote Sens. Lett.
PD SEP 2
PY 2014
VL 5
IS 9
BP 783
EP 792
DI 10.1080/2150704X.2014.967881
PG 10
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA AQ9WW
UT WOS:000343209800002
ER

PT J
AU Marasco, DE
   Hunter, BN
   Culligan, PJ
   Gaffin, SR
   McGillis, WR
AF Marasco, Daniel E.
   Hunter, Betsy N.
   Culligan, Patricia J.
   Gaffin, Stuart R.
   McGillis, Wade R.
TI Quantifying Evapotranspiration from Urban Green Roofs: A Comparison of
   Chamber Measurements with Commonly Used Predictive Methods
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID CENTRAL GREAT PLAINS; BOWEN-RATIO METHOD; ENERGY-BALANCE; WATER-QUALITY;
   HEAT; PERFORMANCE; RUNOFF; EVAPORATION; LYSIMETER; SURFACE
AB Quantifying green roof evapotranspiration (ET) in urban climates is important for assessing environmental benefits, including stormwater runoff attenuation and urban heat island mitigation. In this study, a dynamic chamber method was developed to quantify ET on two extensive green roofs located in New York City, NY. Hourly chamber measurements taken from July 2009 to December 2009 and April 2012 to October 2013 illustrate both diurnal and seasonal variations in ET. Observed monthly total ET depth ranged from 0.22 cm in winter to 15.36 cm in summer. Chamber results were compared to two predictive methods for estimating ET; namely the Penman-based ASCE Standardized Reference Evapotranspiration (ASCE RET) equation, and an energy balance model, both parametrized using on-site environmental conditions. Dynamic chamber ET results were similar to ASCE RET estimates; however, the ASCE RET equation overestimated bottommost ET values during the winter months, and underestimated peak ET values during the summer months. The energy balance method was shown to underestimate ET compared the ASCE RET equation. The work highlights the utility of the chamber method for quantifying green roof evapotranspiration and indicates green roof ET might be better estimated by Penman-based evapotranspiration equations than energy balance methods.
C1 [Marasco, Daniel E.; Culligan, Patricia J.] Columbia Univ, Dept Civil Engn & Engn Mech, New York, NY 10027 USA.
   [Hunter, Betsy N.; McGillis, Wade R.] Columbia Univ, Dept Earth & Environm Engn, New York, NY 10027 USA.
   [Gaffin, Stuart R.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA.
   [Gaffin, Stuart R.] NASA Goddard Inst Space Studies, New York, NY 10027 USA.
   [McGillis, Wade R.] Columbia Univ, Lamont Doherty Earth Observ, New York, NY 10027 USA.
RP Culligan, PJ (reprint author), Columbia Univ, Dept Civil Engn & Engn Mech, 116th St & Broadway, New York, NY 10027 USA.
EM pjc2104@columbia.edu
FU National Science Foundation [CMMI-0928604, DEB-0949387]; NSF Integrative
   Graduate Education and Research Training (IGERT) Fellowship
   [DGE-0903597]; Columbia University Office of Environmental Stewardship;
   United States Postal Service; TectaAmerica
FX This work was supported, in part, by the National Science Foundation
   grants CMMI-0928604 and DEB-0949387. D.M. gratefully acknowledges the
   support of the NSF Integrative Graduate Education and Research Training
   (IGERT) Fellowship DGE-0903597. The authors also wish to thank Columbia
   University Office of Environmental Stewardship, the United States Postal
   Service, and TectaAmerica for their support of this research. Any
   opinions, findings, and conclusions expressed in this paper are those of
   the authors and do not necessarily reflect the views of any supporting
   institution.
NR 60
TC 9
Z9 9
U1 8
U2 71
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
EI 1520-5851
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD SEP 2
PY 2014
VL 48
IS 17
BP 10273
EP 10281
DI 10.1021/es501699h
PG 9
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA AO3KY
UT WOS:000341229300041
PM 25072298
ER

PT J
AU Spiegel, DS
   Fortney, JJ
   Sotin, C
AF Spiegel, David S.
   Fortney, Jonathan J.
   Sotin, Christophe
TI Structure of exoplanets
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
   AMERICA
LA English
DT Article
DE gas giants; hot Jupiters; super-Earths
ID EXTRASOLAR GIANT PLANETS; MASS-RADIUS RELATION; 100 EARTH MASSES; HOT
   JUPITERS; SUPER-EARTHS; TRANSMISSION SPECTRUM; INTERIOR STRUCTURE;
   THERMAL EVOLUTION; OHMIC DISSIPATION; OCEAN-PLANETS
AB The hundreds of exoplanets that have been discovered in the past two decades offer a new perspective on planetary structure. Instead of being the archetypal examples of planets, those of our solar system are merely possible outcomes of planetary system formation and evolution, and conceivably not even especially common outcomes (although this remains an open question). Here, we review the diverse range of interior structures that are both known and speculated to exist in exoplanetary systems-from mostly degenerate objects that are more than 10x as massive as Jupiter, to intermediate-mass Neptune-like objects with large cores and moderate hydrogen/helium envelopes, to rocky objects with roughly the mass of Earth.
C1 [Spiegel, David S.] Inst Adv Study, Sch Nat Sci, Dept Astrophys, Princeton, NJ 08540 USA.
   [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
   [Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Spiegel, DS (reprint author), Inst Adv Study, Sch Nat Sci, Dept Astrophys, Olden Lane, Princeton, NJ 08540 USA.
EM dave@ias.edu
FU National Science Foundation (NSF) [AST-0807444]; Keck Fellowship;
   Association of Members of the Institute for Advanced Study; NSF
   [AST-1010017]; NASA Astrobiology Institute Icy Worlds
FX Support for this work was provided by National Science Foundation (NSF)
   Grant AST-0807444, a Keck Fellowship, Friends of the Institute, and
   Association of Members of the Institute for Advanced Study (to D. S.
   S.); NSF Grant AST-1010017 (to J.F.); and NASA Astrobiology Institute
   Icy Worlds (C.S.).
NR 78
TC 5
Z9 5
U1 4
U2 40
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD SEP 2
PY 2014
VL 111
IS 35
BP 12622
EP 12627
DI 10.1073/pnas.1304206111
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AO3LN
UT WOS:000341230800035
PM 24379369
ER

PT J
AU McKay, CP
AF McKay, Christopher P.
TI Requirements and limits for life in the context of exoplanets
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
   AMERICA
LA English
DT Article
DE extremophiles; Mars; astrobiology
ID CYANOBACTERIUM CHROOCOCCIDIOPSIS; DEINOCOCCUS-RADIODURANS;
   RADIATION-RESISTANCE; IONIZING-RADIATION; LIQUID METHANE; MICROBIAL
   LIFE; ATACAMA DESERT; DEGREES-C; ORIGIN; TITAN
AB The requirements for life on Earth, its elemental composition, and its environmental limits provide a way to assess the habitability of exoplanets. Temperature is key both because of its influence on liquid water and because it can be directly estimated from orbital and climate models of exoplanetary systems. Life can grow and reproduce at temperatures as low as -15 degrees C, and as high as 122 degrees C. Studies of life in extreme deserts show that on a dry world, even a small amount of rain, fog, snow, and even atmospheric humidity can be adequate for photosynthetic production producing a small but detectable microbial community. Life is able to use light at levels less than 10-5 of the solar flux at Earth. UV or ionizing radiation can be tolerated by many microorganisms at very high levels and is unlikely to be life limiting on an exoplanet. Biologically available nitrogen may limit habitability. Levels of O-2 over a few percent on an exoplanet would be consistent with the presence of multicellular organisms and high levels of O-2 on Earth-like worlds indicate oxygenic photosynthesis. Other factors such as pH and salinity are likely to vary and not limit life over an entire planet or moon.
C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP McKay, CP (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
EM chris.mckay@nasa.gov
NR 76
TC 6
Z9 9
U1 10
U2 140
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD SEP 2
PY 2014
VL 111
IS 35
BP 12628
EP 12633
DI 10.1073/pnas.1304212111
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AO3LN
UT WOS:000341230800036
PM 24927538
ER

PT J
AU Batalha, NM
AF Batalha, Natalie M.
TI Exploring exoplanet populations with NASA's Kepler Mission
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
   AMERICA
LA English
DT Article
DE planet detection; transit photometry
ID TRANSIT TIMING OBSERVATIONS; MULTIPLE-PLANET SYSTEMS; SUN-LIKE STAR;
   LOW-DENSITY PLANETS; EARTH-SIZED PLANET; SOLAR-TYPE STARS;
   R-CIRCLE-PLUS; HABITABLE ZONE; TERRESTRIAL PLANETS; ECLIPSING BINARIES
AB The Kepler Mission is exploring the diversity of planets and planetary systems. Its legacy will be a catalog of discoveries sufficient for computing planet occurrence rates as a function of size, orbital period, star type, and insolation flux. The mission has made significant progress toward achieving that goal. Over 3,500 transiting exoplanets have been identified from the analysis of the first 3 y of data, 100 planets of which are in the habitable zone. The catalog has a high reliability rate (85-90% averaged over the period/radius plane), which is improving as follow-up observations continue. Dynamical (e.g., velocimetry and transit timing) and statistical methods have confirmed and characterized hundreds of planets over a large range of sizes and compositions for both single-and multiple-star systems. Population studies suggest that planets abound in our galaxy and that small planets are particularly frequent. Here, I report on the progress Kepler has made measuring the prevalence of exoplanets orbiting within one astronomical unit of their host stars in support of the National Aeronautics and Space Administration's long-term goal of finding habitable environments beyond the solar system.
C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Batalha, NM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Natalie.M.Batalha@nasa.gov
FU NASA's Science Mission Directorate
FX The significant science results based on Kepler data described in this
   volume would not have been possible without the decades of persistence,
   hard work, creativity, and expertise of William Borucki (Principal
   Investigator), Dave Koch (Deputy Principal Investigator), Jon Jenkins
   (Analysis Lead), and Doug Caldwell (Instrument Scientist). Kepler's
   co-Investigators, Science Working Group members, Follow-Up Observers,
   and Participating Scientists (Participating Scientist Program) provide
   critical expertise and analyses that help Kepler meet its baseline
   objectives. The Science Operations Center provides the software pipeline
   for constructing light curves and identifying planet candidates. The
   Science Office, led by Michael Haas, produces the well-vetted and highly
   reliable catalogs that Kepler's planet occurrence rates are derived
   from. This research has made use of the National Aeronautics and Space
   Administration (NASA) Exoplanet Archive, which is operated by the
   California Institute of Technology, under contract with the NASA under
   the Exoplanet Exploration Program. Kepler was competitively selected as
   the 10th Discovery Mission. Funding for this mission is provided by
   NASA's Science Mission Directorate.
NR 93
TC 33
Z9 34
U1 6
U2 69
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD SEP 2
PY 2014
VL 111
IS 35
BP 12647
EP 12654
DI 10.1073/pnas.1304196111
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AO3LN
UT WOS:000341230800039
PM 25049406
ER

PT J
AU Macintosh, B
   Graham, JR
   Ingraham, P
   Konopacky, Q
   Marois, C
   Perrin, M
   Poyneer, L
   Bauman, B
   Barman, T
   Burrows, AS
   Cardwell, A
   Chilcote, J
   De Rosa, RJ
   Dillon, D
   Doyon, R
   Dunn, J
   Erikson, D
   Fitzgerald, MP
   Gavel, D
   Goodsell, S
   Hartung, M
   Hibon, P
   Kalas, P
   Larkin, J
   Maire, J
   Marchis, F
   Marley, MS
   McBride, J
   Millar-Blanchaer, M
   Morzinski, K
   Norton, A
   Oppenheimer, BR
   Palmer, D
   Patience, J
   Pueyo, L
   Rantakyro, F
   Sadakuni, N
   Saddlemyer, L
   Savransky, D
   Serio, A
   Soummer, R
   Sivaramakrishnan, A
   Song, I
   Thomas, S
   Wallace, JK
   Wiktorowicz, S
   Wolff, S
AF Macintosh, Bruce
   Graham, James R.
   Ingraham, Patrick
   Konopacky, Quinn
   Marois, Christian
   Perrin, Marshall
   Poyneer, Lisa
   Bauman, Brian
   Barman, Travis
   Burrows, Adam S.
   Cardwell, Andrew
   Chilcote, Jeffrey
   De Rosa, Robert J.
   Dillon, Daren
   Doyon, Rene
   Dunn, Jennifer
   Erikson, Darren
   Fitzgerald, Michael P.
   Gavel, Donald
   Goodsell, Stephen
   Hartung, Markus
   Hibon, Pascale
   Kalas, Paul
   Larkin, James
   Maire, Jerome
   Marchis, Franck
   Marley, Mark S.
   McBride, James
   Millar-Blanchaer, Max
   Morzinski, Katie
   Norton, Andrew
   Oppenheimer, B. R.
   Palmer, David
   Patience, Jennifer
   Pueyo, Laurent
   Rantakyro, Fredrik
   Sadakuni, Naru
   Saddlemyer, Leslie
   Savransky, Dmitry
   Serio, Andrew
   Soummer, Remi
   Sivaramakrishnan, Anand
   Song, Inseok
   Thomas, Sandrine
   Wallace, J. Kent
   Wiktorowicz, Sloane
   Wolff, Schuyler
TI First light of the Gemini Planet Imager
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
   AMERICA
LA English
DT Article
DE high-contrast imaging; extreme adaptive optics; debris disks
ID ADAPTIVE-OPTICS SYSTEM; POINT-SPREAD FUNCTIONS; BETA-PICTORIS; FINDING
   CAMPAIGN; FOURIER-TRANSFORM; GIANT PLANETS; DEBRIS DISK; HR 8799;
   FREQUENCY; EXOPLANET
AB The Gemini Planet Imager is a dedicated facility for directly imaging and spectroscopically characterizing extrasolar planets. It combines a very high-order adaptive optics system, a diffraction-suppressing coronagraph, and an integral field spectrograph with low spectral resolution but high spatial resolution. Every aspect of the Gemini Planet Imager has been tuned for maximum sensitivity to faint planets near bright stars. During first-light observations, we achieved an estimated H band Strehl ratio of 0.89 and a 5-sigma contrast of 10(6) at 0.75 arcseconds and 10(5) at 0.35 arcseconds. Observations of Beta Pictoris clearly detect the planet, Beta Pictoris b, in a single 60-s exposure with minimal postprocessing. Beta Pictoris b is observed at a separation of 434 +/- 6 milliarcseconds (mas) and position angle 211.8 +/- 0.5 degrees. Fitting the Keplerian orbit of Beta Pic b using the new position together with previous astrometry gives a factor of 3 improvement in most parameters over previous solutions. The planet orbits at a semimajor axis of 9.0(-0.4)(+0.8) AU near the 3:2 resonance with the previously known 6-AU asteroidal belt and is aligned with the inner warped disk. The observations give a 4% probability of a transit of the planet in late 2017.
C1 [Macintosh, Bruce; Poyneer, Lisa; Bauman, Brian; Palmer, David] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA.
   [Macintosh, Bruce; Ingraham, Patrick] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
   [Graham, James R.; Kalas, Paul; McBride, James] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
   [Konopacky, Quinn; Maire, Jerome; Millar-Blanchaer, Max] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
   [Marois, Christian; Dunn, Jennifer; Erikson, Darren; Saddlemyer, Leslie] Natl Res Council Canada Herzberg, Victoria, BC V9E 2E7, Canada.
   [Perrin, Marshall; Pueyo, Laurent; Soummer, Remi; Sivaramakrishnan, Anand] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
   [Barman, Travis] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
   [Burrows, Adam S.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
   [Cardwell, Andrew; Goodsell, Stephen; Hartung, Markus; Hibon, Pascale; Rantakyro, Fredrik; Sadakuni, Naru; Serio, Andrew] Gemini Observ, Hilo, HI 96720 USA.
   [Chilcote, Jeffrey; Fitzgerald, Michael P.; Larkin, James] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
   [De Rosa, Robert J.; Patience, Jennifer] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
   [Dillon, Daren; Gavel, Donald; Norton, Andrew; Wiktorowicz, Sloane] Univ Calif Santa Cruz, Univ Calif Observ Lick Observ, Santa Cruz, CA 95064 USA.
   [Doyon, Rene] Univ Montreal, Observ Mt Megant, Montreal, PQ H3T 1J4, Canada.
   [Doyon, Rene] Univ Montreal, Dept Phys, Montreal, PQ H3T 1J4, Canada.
   [Marchis, Franck] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
   [Marley, Mark S.; Thomas, Sandrine] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Morzinski, Katie] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
   [Oppenheimer, B. R.; Sivaramakrishnan, Anand] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
   [Savransky, Dmitry] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA.
   [Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
   [Wallace, J. Kent] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
   [Wolff, Schuyler] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Macintosh, B (reprint author), Lawrence Livermore Natl Lab, Livermore, CA 94551 USA.
EM bmacintosh@stanford.edu
RI Marley, Mark/I-4704-2013; Savransky, Dmitry/M-1298-2014; 
OI Savransky, Dmitry/0000-0002-8711-7206; Marley, Mark/0000-0002-5251-2943;
   Morzinski, Katie/0000-0002-1384-0063; Fitzgerald,
   Michael/0000-0002-0176-8973
FU Gemini Observatory; National Science Foundation (NSF) Center for
   Adaptive Optics at University of California, Santa Cruz; NSF
   [AST-0909188, AST-1211562]; NASA Origins [NNX11AD21G, NNX10AH31G];
   University of California Office of the President [LFRP-118057]; Dunlap
   Institute, University of Toronto; U.S. Department of Energy by Lawrence
   Livermore National Laboratory [DE-AC52-07NA27344]; California Institute
   of Technology Jet Propulsion Laboratory - NASA through the Sagan
   Fellowship Program
FX We thank the international team of engineers and scientists who worked
   to make GPI a reality. We especially recognize the unique contributions
   of Gary Sommargren, Steven Varlese, Christopher Lockwood, Russell
   Makidon, Murray Fletcher, and Vincent Fesquet, who passed away during
   the course of this project. We acknowledge financial support of the
   Gemini Observatory, the National Science Foundation (NSF) Center for
   Adaptive Optics at University of California, Santa Cruz, the NSF
   (AST-0909188; AST-1211562), NASA Origins (NNX11AD21G and NNX10AH31G),
   the University of California Office of the President (LFRP-118057), and
   the Dunlap Institute, University of Toronto. Portions of this work were
   performed under the auspices of the U.S. Department of Energy by
   Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344
   and under contract with the California Institute of Technology Jet
   Propulsion Laboratory funded by NASA through the Sagan Fellowship
   Program executed by the NASA Exoplanet Science Institute.
NR 51
TC 121
Z9 121
U1 1
U2 4
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD SEP 2
PY 2014
VL 111
IS 35
BP 12661
EP 12666
DI 10.1073/pnas.1304215111
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA AO3LN
UT WOS:000341230800041
PM 24821792
ER

PT J
AU Tombesi, F
   Cappi, M
AF Tombesi, F.
   Cappi, M.
TI On the presence of ultrafast outflows in the WAX sample of Seyfert
   galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE line: identification; galaxies: active; X-rays: galaxies
ID X-RAY-ABSORPTION; ACTIVE GALACTIC NUCLEI; ACCRETION-DISK WINDS;
   RADIO-QUIET AGNS; 3C 111; WARM ABSORBERS; BLACK-HOLE; MULTIWAVELENGTH
   CAMPAIGN; K EMISSION; LINES
AB The study of winds in active galactic nuclei (AGNs) is of utmost importance as they may provide the long sought-after link between the central black hole and the host galaxy, establishing the AGN feedback. Recently, Laha et al. reported the X-ray analysis of a sample of 26 Seyferts observed with XMM-Newton, which are part of the so-called warm absorbers in X-rays (WAX) sample. They claim the non-detection of Fe K absorbers indicative of ultrafast outflows in four observations previously analysed by Tombesi et al. They mainly impute the Tombesi et al. detections to an improper modelling of the underlying continuum in the E = 4-10 keV band. We therefore re-address here the robustness of these detections and we find that the main reason for the claimed non-detections is likely due to their use of single events only spectra, which reduces the total counts by 40 per cent. Performing a re-analysis of the data in the whole E = 0.3-10 keV energy band using their models and spectra including also double events, we find that the blueshifted Fe K absorption lines are indeed detected at > 99 per cent. This work demonstrates the robustness of these detections in XMM-Newton even including complex model components such as reflection, relativistic lines and warm absorbers.
C1 [Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, 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 Tombesi, F (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
EM ftombesi@astro.umd.edu
OI Cappi, Massimo/0000-0001-6966-8920
NR 35
TC 1
Z9 1
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 1
PY 2014
VL 443
IS 1
BP L104
EP L108
DI 10.1093/mnrasl/slu091
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA CL9IP
UT WOS:000357291900022
ER

PT J
AU Cohen, HS
   Mulavara, AP
   Sangi-Haghpeykar, H
   Peters, BT
   Bloomberg, JJ
   Pavlik, VN
AF Cohen, Helen S.
   Mulavara, Ajitkumar P.
   Sangi-Haghpeykar, Haleh
   Peters, Brian T.
   Bloomberg, Jacob J.
   Pavlik, Valory N.
TI Screening People in the Waiting Room for Vestibular Impairments
SO SOUTHERN MEDICAL JOURNAL
LA English
DT Article
DE dizziness; inner ear; public health; screening assessment
ID EVOKED MYOGENIC POTENTIALS; BONE-CONDUCTED VIBRATION; SENSORY
   INTERACTION; MIDLINE FOREHEAD; STANDING BALANCE; HEAD-IMPULSE; TESTS;
   EPIDEMIOLOGY; POPULATION; VERTIGO
AB Objective Primary care physicians need good screening tests of the vestibular system to help them determine whether patients who complain of dizziness should be evaluated for vestibular disorders. The goal of this study was to determine whether current, widely used screening tests of the vestibular system predict subsequent performance on objective diagnostic tests of the vestibular system (ENG).
   Methods Of 300 subjects who were recruited from the waiting room of a primary care clinic and were screened there, 69 subjects subsequently volunteered for ENGs in the otolaryngology department. The screening study included age, history of vertigo, head impulse tests, Dix-Hallpike maneuvers, and the Clinical Test of Sensory Integration and Balance with the head still and the head pitching at 0.33 Hz. The ENG included Dix-Hallpike maneuvers, vestibular-evoked myogenic potentials, bithermal water caloric tests, and low-frequency sinusoids in the rotatory chair in darkness.
   Results The scores on the screening were related to the total ENG, but odds ratios were not significant for some variables, probably because of the small sample size.
   Conclusions A larger sample may have yielded stronger results, but in general the high odds ratios suggest a relation between the ENG score and Dix-Hallpike responses and between the ENG scores and some Clinical Test of Sensory Integration and Balance responses.
C1 Baylor Coll Med, Bobby R Alford Dept Otolaryngol Head & Neck Surg, Houston, TX 77030 USA.
   Baylor Coll Med, Dept Obstet & Gynecol, Houston, TX 77030 USA.
   Baylor Coll Med, Dept Family & Community Med, Houston, TX 77030 USA.
   NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA.
   NASA, Lyndon B Johnson Space Ctr, Wyle Sci Technol & Engn Grp, Houston, TX 77058 USA.
   NASA, Lyndon B Johnson Space Ctr, Neurosci Lab, Houston, TX 77058 USA.
RP Cohen, HS (reprint author), Baylor Coll Med, Dept Otolaryngol, One Baylor Plaza, Houston, TX 77030 USA.
EM hcohen@bcm.edu
FU National Institutes of Health [R01DC009031]; National Space Biomedical
   Research Institute [NASA NCC 9-58]; Agency for Healthcare Research and
   Quality
FX The study was supported by National Institutes of Health grant
   R01DC009031 (HSC) and grants from the National Space Biomedical Research
   Institute through NASA NCC 9-58 (A.P.M. and J.J.B.). V.N.P. has received
   grants from the Agency for Healthcare Research and Quality. The other
   authors have no financial relationships to disclose and no conflicts of
   interest to report.
NR 23
TC 1
Z9 1
U1 0
U2 0
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA
SN 0038-4348
EI 1541-8243
J9 SOUTH MED J
JI South.Med.J.
PD SEP
PY 2014
VL 107
IS 9
BP 549
EP 553
PG 5
WC Medicine, General & Internal
SC General & Internal Medicine
GA CA6VK
UT WOS:000349053700003
PM 25188617
ER

PT J
AU Tarabalka, Y
   Charpiat, G
   Brucker, L
   Menze, BH
AF Tarabalka, Yuliya
   Charpiat, Guillaume
   Brucker, Ludovic
   Menze, Bjoern H.
TI Spatio-Temporal Video Segmentation With Shape Growth or Shrinkage
   Constraint
SO IEEE TRANSACTIONS ON IMAGE PROCESSING
LA English
DT Article
DE Video segmentation; shape growth; graph cut; energy minimization;
   infinite links
ID MARKOV RANDOM-FIELDS; PRIORS; OPTIMIZATION; IMAGES; MODEL; TIME
AB We propose a new method for joint segmentation of monotonously growing or shrinking shapes in a time sequence of noisy images. The task of segmenting the image time series is expressed as an optimization problem using the spatio-temporal graph of pixels, in which we are able to impose the constraint of shape growth or of shrinkage by introducing monodirectional infinite links connecting pixels at the same spatial locations in successive image frames. The globally optimal solution is computed with a graph cut. The performance of the proposed method is validated on three applications: segmentation of melting sea ice floes and of growing burned areas from time series of 2D satellite images, and segmentation of a growing brain tumor from sequences of 3D medical scans. In the latter application, we impose an additional intersequences inclusion constraint by adding directed infinite links between pixels of dependent image structures.
C1 [Tarabalka, Yuliya; Charpiat, Guillaume] Inria Sophia Antipolis Mediteranee, F-06902 Sophia Antipolis, France.
   [Brucker, Ludovic] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA.
   [Menze, Bjoern H.] Tech Univ Munich, Dept Comp Sci, Inst Adv Study, D-80290 Munich, Germany.
RP Tarabalka, Y (reprint author), Inria Sophia Antipolis Mediteranee, F-06902 Sophia Antipolis, France.
EM yuliya.tarabalka@inria.fr; guillaume.charpiat@inria.fr;
   ludovic.brucker@nasa.gov; bjoern.menze@tum.de
RI Brucker, Ludovic/A-8029-2010
OI Brucker, Ludovic/0000-0001-7102-8084
NR 35
TC 4
Z9 4
U1 0
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1057-7149
EI 1941-0042
J9 IEEE T IMAGE PROCESS
JI IEEE Trans. Image Process.
PD SEP
PY 2014
VL 23
IS 9
BP 3829
EP 3840
DI 10.1109/TIP.2014.2336544
PG 12
WC Computer Science, Artificial Intelligence; Engineering, Electrical &
   Electronic
SC Computer Science; Engineering
GA AZ6YT
UT WOS:000348366100007
PM 25020092
ER

PT J
AU Kim, HC
   Son, S
   Montagna, P
   Spiering, B
   Nam, J
AF Kim, Hae-Cheol
   Son, Seunghyun
   Montagna, Paul
   Spiering, Bruce
   Nam, Jungho
TI Linkage between Freshwater Inflow and Primary Productivity in Texas
   Estuaries: Downscaling Effects of Climate Variability
SO JOURNAL OF COASTAL RESEARCH
LA English
DT Article
DE ENSO; MODIS; tele-connection; climatic gradient; chlorophyll; ecosystem
   responses
ID SEA-SURFACE TEMPERATURE; NET ECOSYSTEM METABOLISM; LAVACA-COLORADO
   ESTUARY; LONG-TERM TRENDS; SOUTHERN-OSCILLATION; MISSISSIPPI RIVER;
   COASTAL EUTROPHICATION; MARINE ECOSYSTEMS; NITROGEN-CYCLE; CHESAPEAKE
   BAY
AB The estuaries of Texas are lagoons that lie in a climatic gradient in the northwestern Gulf of Mexico (GOM). Estuaries located in the northeastern part of the Texas coast receive more rainfall than estuaries in the southwestern part, and consequently greater runoff and concomitant freshwater inflow. Extreme inter-annual variability of precipitation caused by El Nino Southern Oscillation (ENSO) events is another characteristic of the Texas coast. During El Nino periods, salinities in Texas estuaries decrease because of increased precipitation and increased freshwater inflow to the coast. During La Nina periods, salinities increase due to drier climatic conditions and reduced freshwater inflow. The combination of the climatic gradient and temporal variability of freshwater inflow drive changes in the frequency, timing, duration, and magnitude of river flows to coastal waters, which in turn control the salinity, nutrients, organic matter, and sediments in Texas estuaries. Chlorophyll biomass, as an indicator of primary production, was estimated from Moderate Resolution Imaging Spectroradiometer (MODIS) data from July 2002 to December 2011 for all Texas estuaries. The climate patterns in the Pacific Ocean delivers a cascading signal via freshwater inflow changes to estuaries that effects primary production subsequently. The maximum correlation was found at the 5th lag (month) with correlation coefficient (rho) being 0.45 (NINO3.4 is fixed as a reference). The combination of the local climatic gradient and quasi-periodic natural variability in ENSO has been influencing estuarine ecosystem dynamics over decadal scales in this region. The present study demonstrates that freshwater inflow is an important driver in maintaining primary productivity of Texas estuaries, which is required to maintain estuarine health and sustainability.
C1 [Kim, Hae-Cheol] NOAA, IM Syst Grp, Environm Modeling Ctr, NCEP, College Pk, MD 20740 USA.
   [Son, Seunghyun] Colorado State Univ, Cooperat Inst Res Atmospher, Ft Collins, CO 80523 USA.
   [Montagna, Paul] Texas A&M Univ Corpus Christi, Harte Res Inst Gulf Mexico Studies, Corpus Christi, TX 78412 USA.
   [Spiering, Bruce] NASA, Appl Sci & Technol Project Off, SSC, Stennis Space Ctr, MS 39529 USA.
   [Nam, Jungho] Korea Maritime Inst, Seoul, South Korea.
RP Nam, J (reprint author), Korea Maritime Inst, Seoul, South Korea.
EM jhnam@kmi.re.kr
FU Korea Maritime Institute (KMI); NOAA, Office of Education Educational
   Partnership Program [NA11SEC4810001]
FX The authors are grateful to anonymous reviewers for their constructive
   comments and suggestion. This publication was made possible, in part, by
   Korea Maritime Institute (KMI) as part of a funded research, "Ecological
   and Socio-Economic Impacts of Watershed Development on Coastal and
   Marine Areas" and, in part, by NOAA, Office of Education Educational
   Partnership Program award (NA11SEC4810001). Computational facilities
   were supported by Harte Research Institute and National Centers for
   Environmental Prediction at NOAA. Its contents do not necessarily
   represent the official views of the U.S. Department of Commerce,
   National Oceanic and Atmospheric Administration.
NR 59
TC 1
Z9 1
U1 2
U2 40
PU COASTAL EDUCATION & RESEARCH FOUNDATION
PI LAWRENCE
PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA
SN 0749-0208
EI 1551-5036
J9 J COASTAL RES
JI J. Coast. Res.
PD FAL
PY 2014
SI 68
BP 65
EP 73
DI 10.2112/SI68-009.1
PG 9
WC Environmental Sciences; Geography, Physical; Geosciences,
   Multidisciplinary
SC Environmental Sciences & Ecology; Physical Geography; Geology
GA AX8FM
UT WOS:000347145600010
ER

PT J
AU Smith, JW
   Jenkins, GS
   Pickering, KE
AF Smith, Jonathan W.
   Jenkins, Gregory S.
   Pickering, Kenneth E.
TI WRF-Chem model estimates of equatorial Atlantic Ocean tropospheric ozone
   increases via June 2006 African biomass burning ozone precursor
   transport
SO JOURNAL OF ATMOSPHERIC CHEMISTRY
LA English
DT Article
DE Biomass burning; Lightning-induced nitrogen oxides; Inter-hemispheric
   transport; Intra-hemispheric; Gulf of Guinea; Detrainment
ID TROPICAL ATLANTIC; WEST-AFRICA; SUMMER MONSOON; AMMA; FIELD; PART;
   ASSIMILATION; CONVECTION; EMISSIONS; PATHWAYS
AB Long-range horizontal and local vertical transport of biomass burning ozone precursors (i.e. carbon monoxide and nitrogen oxides) from Central Africa are simulated for June 2006. Twenty-kilometer resolution combined meteorological and chemical simulations examine transport pathways, spatial distribution, and quantities of ozone precursors and ozone. Results suggest that due to biomass burning, ozone mixing ratios increase by 28-33 parts per billion by volume in the lower troposphere (850 hecto-Pascals) over the Atlantic Ocean west of Central Africa during June. The inter-hemispheric transport of biomass burning emissions from Central Africa subsides over the Gulf of Guinea with a northward extent of approximately 2-5A degrees N. In the lower troposphere, ozone mixing ratio increases decrease from 28 parts per billion by volume in the southern Gulf of Guinea to 2-3 parts per billion by volume on the Gulf of Guinea Coast. There is middle and upper tropospheric ozone enhancement of 6-12 parts per billion over the Equatorial Atlantic Ocean which is the result of convective detrainment of ozone precursors from deep convection on the Gulf of Guinea Coast followed by transport that propagates around a broad anticyclone. The model ozone produced by biomass burning emissions is less than the observed implying that lightning-induced nitrogen oxide emissions, which are not included in this simulation, are a significant tropospheric ozone source for the eastern Equatorial Atlantic Ocean.
C1 [Smith, Jonathan W.] NOAA NCWCP, NOAA NESDIS STAR SMCD, Natl Res Council Postdoctoral Res Associateship, College Pk, MD 20741 USA.
   [Jenkins, Gregory S.] Howard Univ, Dept Phys & Astron, Washington, DC 20001 USA.
   [Jenkins, Gregory S.] Howard Univ, Howard Univ Program Atmospher Sci, Washington, DC 20001 USA.
   [Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
RP Smith, JW (reprint author), NOAA NCWCP, NOAA NESDIS STAR SMCD, Natl Res Council Postdoctoral Res Associateship, 2844,5830 Univ Res Ct, College Pk, MD 20741 USA.
EM jonathan.smith@noaa.gov
RI Pickering, Kenneth/E-6274-2012
FU NSF ATM [621159]; National Academy of Science-National Research Council
   Postdoctoral Associateship; Earth Science Division at Goddard Space
   Flight Center (GSFC)
FX This work is funded by NSF ATM Grant # 621159 and the National Academy
   of Science-National Research Council Postdoctoral Associateship. From
   2009 to 2013, the work was partially funded by the Earth Science
   Division at Goddard Space Flight Center (GSFC). The simulations were
   completed on the Discover supercomputer at the NASA Center for Climate
   Simulation at GSFC. Paul Novelli of the NOAA/Earth System Research
   Laboratory/Global Monitoring Division provided CCGG flask point surface
   CO mixing ratio data. Nickolay Krotkov and Lok Lamsal in the Atmospheric
   Chemistry and Dynamics Laboratory at GSFC processed and provided gridded
   NO<INF>2</INF> OMI data. I thank Mary Barth of the NCAR for a
   constructive critique of the work in its early stages.
NR 49
TC 0
Z9 0
U1 2
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 2014
VL 71
IS 3
BP 225
EP 251
DI 10.1007/s10874-014-9293-x
PG 27
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA AW4IW
UT WOS:000346245600004
ER

PT J
AU Meier, WN
   Hovelsrud, GK
   van Oort, BEH
   Key, JR
   Kovacs, KM
   Michel, C
   Haas, C
   Granskog, MA
   Gerland, S
   Perovich, DK
   Makshtas, A
   Reist, JD
AF Meier, Walter N.
   Hovelsrud, Greta K.
   van Oort, Bob E. H.
   Key, Jeffrey R.
   Kovacs, Kit M.
   Michel, Christine
   Haas, Christian
   Granskog, Mats A.
   Gerland, Sebastian
   Perovich, Donald K.
   Makshtas, Alexander
   Reist, James D.
TI Arctic sea ice in transformation: A review of recent observed changes
   and impacts on biology and human activity
SO REVIEWS OF GEOPHYSICS
LA English
DT Review
ID WESTERN HUDSON-BAY; SUBSURFACE CHLOROPHYLL MAXIMA; POLAR BEAR
   POPULATIONS; SOUTHERN BEAUFORT SEA; GLOBAL CLIMATE MODELS; MARINE
   MAMMALS; FRAM STRAIT; FOOD AVAILABILITY; BELUGA WHALES; TIPPING POINT
AB Sea ice in the Arctic is one of the most rapidly changing components of the global climate system. Over the past few decades, summer areal extent has declined over 30%, and all months show statistically significant declining trends. New satellite missions and techniques have greatly expanded information on sea ice thickness, but many uncertainties remain in the satellite data and long-term records are sparse. However, thickness observations and other satellite-derived data indicate a 40% decline in thickness, due in large part to the loss of thicker, older ice cover. The changes in sea ice are happening faster than models have projected. With continued increasing temperatures, summer ice-free conditions are likely sometime in the coming decades, though there are substantial uncertainties in the exact timing and high interannual variability will remain as sea ice decreases. The changes in Arctic sea ice are already having an impact on flora and fauna in the Arctic. Some species will face increasing challenges in the future, while new habitat will open up for other species. The changes are also affecting people living and working in the Arctic. Native communities are facing challenges to their traditional ways of life, while new opportunities open for shipping, fishing, and natural resource extraction. Significant progress has been made in recent years in understanding of Arctic sea ice and its role in climate, the ecosystem, and human activities. However, significant challenges remain in furthering the knowledge of the processes, impacts, and future evolution of the system.
C1 [Meier, Walter N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Hovelsrud, Greta K.; van Oort, Bob E. H.] Ctr Int Climate & Environm Res Oslo, Oslo, Norway.
   [Hovelsrud, Greta K.] Nordland Res Inst, Bodo, Norway.
   [Key, Jeffrey R.] NOAA, Madison, WI USA.
   [Kovacs, Kit M.; Granskog, Mats A.; Gerland, Sebastian] Norwegian Polar Res Inst, Tromso, Norway.
   [Michel, Christine; Reist, James D.] Fisheries & Oceans Canada, Winnipeg, MB, Canada.
   [Haas, Christian] Univ Alberta, Dept Earth & Atmospher Sci & Geophys, Edmonton, AB, Canada.
   [Perovich, Donald K.] US Army Cold Reg Res & Engn Lab, Hanover, NH USA.
   [Makshtas, Alexander] Arctic & Antarctic Res Inst, St Petersburg 199226, Russia.
RP Meier, WN (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM walt.meier@nasa.gov
RI Key, Jeffrey/F-5597-2010; Haas, Christian/L-5279-2016; 
OI Key, Jeffrey/0000-0001-6109-3050; Haas, Christian/0000-0002-7674-3500;
   Meier, Walter/0000-0003-2857-0550
FU Arctic Council; NASA; NOAA; U.S. Department of Defense; Norwegian Polar
   Institute; Fisheries and Oceans Canada
FX This work was supported by the Arctic Council and the agencies employing
   and funding the authors including NASA, NOAA, U.S. Department of
   Defense, the Norwegian Polar Institute, and Fisheries and Oceans Canada.
   The views, opinions, and findings contained in this report are those of
   the author(s) and should not be construed as an official National
   Oceanic and Atmospheric Administration or U.S. Government position,
   policy, or decision.
NR 270
TC 40
Z9 43
U1 26
U2 185
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 2014
VL 52
IS 3
BP 185
EP 217
DI 10.1002/2013RG000431
PG 33
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AU5MI
UT WOS:000345650700001
ER

PT J
AU Stammer, D
   Ray, RD
   Andersen, OB
   Arbic, BK
   Bosch, W
   Carrere, L
   Cheng, Y
   Chinn, DS
   Dushaw, BD
   Egbert, GD
   Erofeeva, SY
   Fok, HS
   Green, JAM
   Griffiths, S
   King, MA
   Lapin, V
   Lemoine, FG
   Luthcke, SB
   Lyard, F
   Morison, J
   Muller, M
   Padman, L
   Richman, JG
   Shriver, JF
   Shum, CK
   Taguchi, E
   Yi, Y
AF Stammer, D.
   Ray, R. D.
   Andersen, O. B.
   Arbic, B. K.
   Bosch, W.
   Carrere, L.
   Cheng, Y.
   Chinn, D. S.
   Dushaw, B. D.
   Egbert, G. D.
   Erofeeva, S. Y.
   Fok, H. S.
   Green, J. A. M.
   Griffiths, S.
   King, M. A.
   Lapin, V.
   Lemoine, F. G.
   Luthcke, S. B.
   Lyard, F.
   Morison, J.
   Mueller, M.
   Padman, L.
   Richman, J. G.
   Shriver, J. F.
   Shum, C. K.
   Taguchi, E.
   Yi, Y.
TI Accuracy assessment of global barotropic ocean tide models
SO REVIEWS OF GEOPHYSICS
LA English
DT Review
ID RECIPROCAL ACOUSTIC TRANSMISSIONS; NORTHWEST EUROPEAN SHELF;
   CURRENT-METER RECORDS; SHALLOW-WATER TIDES; INTERNAL TIDES; DEEP-OCEAN;
   TOPEX/POSEIDON ALTIMETRY; SATELLITE ALTIMETRY; GENERAL-CIRCULATION;
   ENERGY-DISSIPATION
AB The accuracy of state-of-the-art global barotropic tide models is assessed using bottom pressure data, coastal tide gauges, satellite altimetry, various geodetic data on Antarctic ice shelves, and independent tracked satellite orbit perturbations. Tide models under review include empirical, purely hydrodynamic ("forward"), and assimilative dynamical, i.e., constrained by observations. Ten dominant tidal constituents in the diurnal, semidiurnal, and quarter-diurnal bands are considered. Since the last major model comparison project in 1997, models have improved markedly, especially in shallow-water regions and also in the deep ocean. The root-sum-square differences between tide observations and the best models for eight major constituents are approximately 0.9, 5.0, and 6.5 cm for pelagic, shelf, and coastal conditions, respectively. Large intermodel discrepancies occur in high latitudes, but testing in those regions is impeded by the paucity of high-quality in situ tide records. Long-wavelength components of models tested by analyzing satellite laser ranging measurements suggest that several models are comparably accurate for use in precise orbit determination, but analyses of GRACE intersatellite ranging data show that all models are still imperfect on basin and subbasin scales, especially near Antarctica. For the M-2 constituent, errors in purely hydrodynamic models are now almost comparable to the 1980-era Schwiderski empirical solution, indicating marked advancement in dynamical modeling. Assessing model accuracy using tidal currents remains problematic owing to uncertainties in in situ current meter estimates and the inability to isolate the barotropic mode. Velocity tests against both acoustic tomography and current meters do confirm that assimilative models perform better than purely hydrodynamic models.
C1 [Stammer, D.; Taguchi, E.] Univ Hamburg, Hamburg, Germany.
   [Ray, R. D.; Lemoine, F. G.; Luthcke, S. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Andersen, O. B.] Tech Univ Denmark, DTU Space, Copenhagen, Denmark.
   [Arbic, B. K.; Dushaw, B. D.] Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA.
   [Bosch, W.] Deutsches Geodat Forschungsinst, Munich, Germany.
   [Carrere, L.; Lyard, F.] Observ Midi Pyrenees, UMR 5566, LEGOS, F-31400 Toulouse, France.
   [Cheng, Y.] Nanjing Univ Informat Sci & Technol, Sch Marine Sci, Nanjing, Jiangsu, Peoples R China.
   [Chinn, D. S.] NASA GSFC, SGT Inc, Greenbelt, MD USA.
   [Egbert, G. D.; Erofeeva, S. Y.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
   [Fok, H. S.] Wuhan Univ, Sch Geodesy & Geomat, Wuhan 430072, Peoples R China.
   [Fok, H. S.; Shum, C. K.; Yi, Y.] Ohio State Univ, Div Geodet Sci, Sch Earth Sci, Columbus, OH 43210 USA.
   [Green, J. A. M.] Bangor Univ, Sch Ocean Sci, Menai Bridge, Gwynedd, Wales.
   [Griffiths, S.; Lapin, V.] Univ Leeds, Dept Appl Math, Leeds LS2 9JT, W Yorkshire, England.
   [King, M. A.] Univ Tasmania, Sch Land & Food, Surveying & Spatial Sci Grp, Hobart, Tas, Australia.
   [Morison, J.] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.
   [Mueller, M.] Norwegian Meteorol Inst, Oslo, Norway.
   [Padman, L.] Earth & Space Res, Corvallis, OR USA.
   [Richman, J. G.; Shriver, J. F.] Naval Res Lab, Oceanog Div, Stennis Space Ctr, MS USA.
   [Shum, C. K.] Chinese Acad Sci, Inst Geodesy & Geophys, Wuhan, Peoples R China.
RP Stammer, D (reprint author), Univ Hamburg, Martinistr 52, Hamburg, Germany.
EM detlef.stammer@zmaw.de
RI Lemoine, Frank/D-1215-2013; Griffiths, Stephen/A-6440-2008; King,
   Matt/B-4622-2008; Ray, Richard/D-1034-2012; Andersen, Ole /H-7481-2016; 
OI Griffiths, Stephen/0000-0002-4654-2636; King, Matt/0000-0001-5611-9498;
   Andersen, Ole /0000-0002-6685-3415; Egbert, Gary/0000-0003-1276-8538;
   Arbic, Brian K/0000-0002-7969-2294
NR 124
TC 47
Z9 49
U1 7
U2 33
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 2014
VL 52
IS 3
BP 243
EP 282
DI 10.1002/2014RG000450
PG 40
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AU5MI
UT WOS:000345650700003
ER

PT J
AU Grindrod, PM
   Warner, NH
AF Grindrod, P. M.
   Warner, N. H.
TI Erosion rate and previous extent of interior layered deposits on Mars
   revealed by obstructed landslides
SO GEOLOGY
LA English
DT Article
ID VALLES-MARINERIS; STABILITY; HISTORY; WIND; ICE
AB We describe interior layered deposits on Mars that have obstructed landslides before undergoing retreat by as much as 2 km. These landslides differ from typical Martian examples in that their toe height increases by as much as 500 m in a distinctive frontal scarp that mimics the shape of the layered deposits. By using crater statistics to constrain the formation ages of the individual landslides to between ca. 200 and 400 Ma, we conclude that the retreat of the interior layered deposits was rapid, requiring erosion rates of between 1200 and 2300 nm yr(-1). We suggest that the interior layered deposits are either extremely friable, if eroded strictly by wind, or composed of a material whose degradation has been enhanced by ice sublimation. These erosion rates also confirm that the interior layered deposits have been in a state of net degradation over the past 400 m.y., suggesting that the process that caused net deposition in the past has ceased or slowed substantially on Mars relative to erosion. Our results imply that interior layered deposits with a similar morphology across Mars, including the mound in Gale Crater, have probably undergone similar rapid erosion and retreat, suggesting that their total modern volume underrepresents the depositional record and thus sedimentary history of Mars.
C1 [Grindrod, P. M.] Univ London, Dept Earth & Planetary Sci, Birkbeck, London WC1E 7HX, England.
   [Grindrod, P. M.] Ctr Planetary Sci UCL Birkbeck, London WC1E 6BT, England.
   [Warner, N. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Grindrod, PM (reprint author), Univ London, Dept Earth & Planetary Sci, Birkbeck, Malet St, London WC1E 7HX, England.
EM p.grindrod@ucl.ac.uk
RI Grindrod, Peter/F-5819-2011
OI Grindrod, Peter/0000-0002-0934-5131
FU UK Space Agency Aurora Fellowship through the Science and Technology
   Facilities Council [T/J005215/1, ST/L00254X/1]
FX Grindrod is funded by a UK Space Agency Aurora Fellowship through the
   Science and Technology Facilities Council (grants ST/J005215/1 and
   ST/L00254X/1). The stereo digital terrain model processing was carried
   out at the UK NASA RPIF (Regional Planetary Image Facility) at
   University College London. We thank Annie Howington-Kraus at the U.S.
   Geological Survey for ongoing help in producing stereo digital terrain
   models. We also thank Paul Niles and an anonymous reviewer for
   thoughtful comments that strengthened the study.
NR 23
TC 8
Z9 8
U1 0
U2 3
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 SEP
PY 2014
VL 42
IS 9
BP 795
EP 798
DI 10.1130/G35790.1
PG 4
WC Geology
SC Geology
GA AU1DU
UT WOS:000345362100015
ER

PT J
AU Le Vine, DM
   Dinnat, EP
   Lagerloef, GSE
   de Matthaeis, P
   Abraham, S
   Utku, C
   Kao, H
AF Le Vine, D. M.
   Dinnat, E. P.
   Lagerloef, G. S. E.
   de Matthaeis, P.
   Abraham, S.
   Utku, C.
   Kao, H.
TI Aquarius: Status and recent results
SO RADIO SCIENCE
LA English
DT Article
ID BAND RADIOMETER/SCATTEROMETER OBSERVATIONS; SEA-SURFACE SALINITY; 3RD
   STOKES PARAMETER; INTERFERENCE MITIGATION; POLAR-REGIONS; SPACE;
   RETRIEVALS; RADIOMETER; MISSION
AB Aquarius is a combination active/passive instrument at L band designed to map sea surface salinity globally from space. The radiometer (passive) is the primary instrument for retrieving salinity, and the scatterometer (active) provides information to correct for a major source of error, sea surface roughness (waves). In addition, the radiometer includes a number of special features designed to meet the goal for this challenging measurement, including measurement of the third Stokes parameter to help with the correction for Faraday rotation and rapid sampling to help with the mitigation of radio frequency interference. Aquarius was launched on 10 June 2011 aboard the Aquarius/SAC-D observatory and has been working well. The salinity retrieval continues to improve, and the special features suggest the potential for new applications of remote sensing from space at L band.
C1 [Le Vine, D. M.; Dinnat, E. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Dinnat, E. P.] Chapman Univ, Sch Earth & Environm Sci, Orange, CA USA.
   [Lagerloef, G. S. E.; Kao, H.] Earth & Space Res, Seattle, WA USA.
   [de Matthaeis, P.; Utku, C.] NASA, Goddard Space Flight Ctr, GESTAR, Greenbelt, MD USA.
   [Abraham, S.] NASA, Goddard Space Flight Ctr, Wyle, Greenbelt, MD USA.
RP Le Vine, DM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM david.m.levine@nasa.gov
RI Dinnat, Emmanuel/D-7064-2012
OI Dinnat, Emmanuel/0000-0001-9003-1182
NR 37
TC 7
Z9 7
U1 1
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
EI 1944-799X
J9 RADIO SCI
JI Radio Sci.
PD SEP
PY 2014
VL 49
IS 9
BP 709
EP 720
DI 10.1002/2014RS005505
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences; Remote Sensing; Telecommunications
GA AU0PM
UT WOS:000345325800002
ER

PT J
AU Hoerling, M
   Wolter, K
   Perlwitz, J
   Quan, XW
   Eischeid, J
   Wang, HL
   Schubert, S
   Diaz, H
   Dole, R
AF Hoerling, Martin
   Wolter, Klaus
   Perlwitz, Judith
   Quan, Xiaowei
   Eischeid, Jon
   Wang, Hailan
   Schubert, Siegfried
   Diaz, Henry
   Dole, Randall
TI NORTHEAST COLORADO EXTREME RAINS INTERPRETED IN A CLIMATE CHANGE CONTEXT
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
AB The probability for an extreme five-day September rainfall event over northeast Colorado, as was observed in early September 2013, has likely decreased due to climate change.
C1 [Hoerling, Martin; Dole, Randall] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
   [Wolter, Klaus; Perlwitz, Judith; Quan, Xiaowei; Eischeid, Jon; Diaz, Henry] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
   [Wang, Hailan] Sci Syst & Applicat Inc, NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA.
   [Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Hoerling, M (reprint author), NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
RI Wolter, Klaus/D-5988-2015; Perlwitz, Judith/B-7201-2008
OI Perlwitz, Judith/0000-0003-4061-2442
NR 0
TC 6
Z9 6
U1 0
U2 7
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 2014
VL 95
IS 9
SU S
BP S15
EP S18
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AT3FD
UT WOS:000344820500005
ER

PT J
AU Wang, H
   Schubert, S
AF Wang, Hailan
   Schubert, Siegfried
TI CAUSES OF THE EXTREME DRY CONDITIONS OVER CALIFORNIA DURING EARLY 2013
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
AB The 2013 SST anomalies produced a predilection for California drought, whereas the long-term warming trend appears to make no appreciable contribution because of the counteraction between its dynamical and thermodynamic effects.
C1 [Wang, Hailan] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA.
   [Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Wang, HL (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA.
NR 0
TC 26
Z9 27
U1 1
U2 30
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 2014
VL 95
IS 9
SU S
BP S7
EP S11
PG 5
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AT3FD
UT WOS:000344820500003
ER

PT J
AU Lau, KY
   Lutes, GF
AF Lau, Kam Y.
   Lutes, George F.
TI Ultra-Stable RF-Over-Fiber Transport Enables NASA Ground-Based Deep
   Space Tracking Antenna Arrays and Space-Borne Earth Mapping Radar
SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE
LA English
DT Article
C1 [Lau, Kam Y.] Univ Calif Berkeley, Dept EECS, Berkeley, CA 94720 USA.
   [Lutes, George F.] NASA Jet Prop Lab, Deep Space Network, Pasadena, CA USA.
RP Lau, KY (reprint author), Univ Calif Berkeley, 253 Cary Hall, Berkeley, CA 94720 USA.
EM klau@eecs.berkeley.edu
FU IEEE Aerospace and Systems Society
FX The authors are grateful to have had the opportunity to work at the NASA
   Jet Propulsion Laboratory and to have contributed in a small way to the
   nation's deep space exploration effort. We would like to thank our past
   and present colleagues in the FTS Group at the NASA JPL for their
   contributions to the work described in this article. We thank the
   Interplanetary Network Directorate at JPL for supporting this work. We
   are also immensely grateful to the IEEE Aerospace and Systems Society
   for recognizing us with the prestigious Pioneer Award for this work done
   more than 30 years ago. We are at the same time honored and humbled to
   be in the company of the many past honorees of this award who have
   contributed to establishing the frontier of the aerospace electronics
   industry as we know it today.
NR 22
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 0885-8985
EI 1557-959X
J9 IEEE AERO EL SYS MAG
JI IEEE Aerosp. Electron. Syst. Mag.
PD SEP
PY 2014
VL 29
IS 9
BP 34
EP 41
DI 10.1109/MAES.2014.140080
PG 8
WC Engineering, Aerospace; Engineering, Electrical & Electronic
SC Engineering
GA AT5MZ
UT WOS:000344988300005
ER

PT J
AU Chang, WM
   Tan, SR
   Lemmetyinen, J
   Tsang, L
   Xu, XL
   Yueh, SH
AF Chang, Wenmo
   Tan, Shurun
   Lemmetyinen, Juha
   Tsang, Leung
   Xu, Xiaolan
   Yueh, Simon H.
TI Dense Media Radiative Transfer Applied to SnowScat and SnowSAR
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
   SENSING
LA English
DT Article; Proceedings Paper
CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS)
CY JUL 21-26, 2013
CL Melbourne, AUSTRALIA
SP IEEE, Inst Elect & Elect Engineers, Geoscience & Remote Sensing Soc
DE Bicontinuous; dense media radiative transfer (DMRT); quasi-crystalline
   approximation (QCA); remote sensing of snow; SnowSAR; SnowScat
ID MICROWAVE EMISSION MODEL; SURFACE-AREA; ELECTROMAGNETIC-WAVES; INFRARED
   REFLECTANCE; LAYERED SNOWPACKS; WATER EQUIVALENT; GRANULAR MEDIA;
   SCATTERING; APPROXIMATION; ADSORPTION
AB The dense media radiative transfer (DMRT) theory is applied to data analysis of recent measurements of multifrequency microwave backscatter from the snow cover on earth. Measurement includes ground-based campaign (SnowScat) and airborne mission (SnowSAR). Both the quasi-crystalline approximation (QCA) model and the bicontinuous model are used for a multilayer snow medium. Two size parameters are used for both models. Grain size and stickiness parameter are used for QCA model. The bicontinuous model has two parameters: the mean wave number <zeta > and the parameter b. The mean wave number <zeta > corresponds to the inverse of the grain size, while the b parameter controls the width of the wave number distribution and is related to the clustering property. The bicontinuous model is used to generate the microstructures of snow by computer, and Maxwell equations are solved numerically for each sample of computer-generated structure to calculate the extinction coefficient and the phase matrix. Other geometric descriptors of the bicontinuous medium include correlation functions and specific surface areas, both of which can be calculated from the parameters <zeta > and b. In making comparisons, we use ground measurements of specific surface area, grain size, densities, and layering of snow cover as input for the theoretical models. The geometric properties and the scattering properties of the bicontinuous model are also compared with past models. In making the multifrequency comparisons, we use the same physical parameters of all three frequencies: 1) X band; 2) Ku bands of 13.3 GHz; and 3) 16.7 GHz. It is emphasized that the DMRT models provide frequency, size, and angular dependence that depart from the classical model of Rayleigh scattering and are in better agreement with experimental observations.
C1 [Chang, Wenmo; Tan, Shurun; Tsang, Leung] Univ Washington, Dept Elect Engn, Seattle, WA 98105 USA.
   [Lemmetyinen, Juha] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
   [Xu, Xiaolan; Yueh, Simon H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Chang, WM (reprint author), Univ Washington, Dept Elect Engn, Seattle, WA 98105 USA.
EM wmchang@uw.edu
RI Lemmetyinen, Juha/B-3739-2016
OI Lemmetyinen, Juha/0000-0003-4434-9696
FU National Aeronautics and Space Administration (NASA) [NNX11AK41G]
FX This work was supported by the National Aeronautics and Space
   Administration (NASA) under Grant NNX11AK41G.
NR 41
TC 12
Z9 12
U1 2
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 2014
VL 7
IS 9
SI SI
BP 3811
EP 3825
DI 10.1109/JSTARS.2014.2343519
PG 15
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
   Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
   Photographic Technology
GA AT5ON
UT WOS:000344992200014
ER

PT J
AU Kubota, T
   Yoshida, N
   Urita, S
   Iguchi, T
   Seto, S
   Meneghini, R
   Awaka, J
   Hanado, H
   Kida, S
   Oki, R
AF Kubota, Takuji
   Yoshida, Naofumi
   Urita, Shinji
   Iguchi, Toshio
   Seto, Shinta
   Meneghini, Robert
   Awaka, Jun
   Hanado, Hiroshi
   Kida, Satoshi
   Oki, Riko
TI Evaluation of Precipitation Estimates by at-Launch Codes of GPM/DPR
   Algorithms Using Synthetic Data from TRMM/PR Observations
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
   SENSING
LA English
DT Article; Proceedings Paper
CT IEEE International Geoscience and Remote Sensing Symposium (IGARSS)
CY JUL 21-26, 2013
CL Melbourne, AUSTRALIA
SP IEEE, Inst Elect & Elect Engineers, Geoscience & Remote Sensing Soc
DE Algorithms; attenuation; Global Precipitation Measurement (GPM); rain;
   simulation; snow; spaceborne radar; Tropical Rainfall Measuring Mission
   (TRMM)
ID SURFACE REFERENCE TECHNIQUE; NONUNIFORM BEAMFILLING CORRECTION; RADAR
   RAINFALL MEASUREMENT; LEAF-AREA INDEX; RETRIEVAL ALGORITHM; KA-BAND;
   MICROWAVE RADIOMETERS; SATELLITE SIMULATOR; PROFILING ALGORITHM;
   CROSS-SECTIONS
AB The Global Precipitation Measurement (GPM) Core Observatory will carry a Dual-frequency Precipitation Radar (DPR) consisting of a Ku-band precipitation radar (KuPR) and a Ka-band precipitation radar (KaPR). In this study, "at-launch" codes of DPR precipitation algorithms, which will be used in GPM ground systems at launch, were evaluated using synthetic data based upon the Tropical Rainfall Measuring Mission (TRMM) Precipitation Radar (PR) data. Results from the codes (Version 4.20131010) of the KuPR-only, KaPR-only, and DPR algorithms were compared with "true values" calculated based upon drop size distributions assumed in the synthetic data and standard results from the TRMM algorithms at an altitude of 2 km over the ocean. The results indicate that the total precipitation amounts during April 2011 from the KuPR and DPR algorithms are similar to the true values, whereas the estimates from the KaPR data are underestimated. Moreover, the DPR estimates yielded smaller precipitation rates for rates less than about 10 mm/h and greater precipitation rates above 10 mm/h. Underestimation of the KaPR estimates was analyzed in terms of measured radar reflectivity (Z(m)) of the KaPR at an altitude of 2 km. The underestimation of the KaPR data was most pronounced during strong precipitation events of Z(m) < 18 dBZ (high attenuation cases) over heavy precipitation areas in the Tropics, whereas the underestimation was less pronounced when the Z(m) > 26 dBZ (moderate attenuation cases). The results suggest that the underestimation is caused by a problem in the attenuation correction method, which was verified by the improved codes.
C1 [Kubota, Takuji; Kida, Satoshi; Oki, Riko] Japan Aerosp Explorat Agcy, Earth Observat Res Ctr, Tsukuba, Ibaraki 3058505, Japan.
   [Yoshida, Naofumi; Urita, Shinji] Remote Sensing Technol Ctr Japan, Tsukuba, Ibaraki 3058505, Japan.
   [Iguchi, Toshio; Hanado, Hiroshi] Natl Inst Informat & Commun Technol, Appl Electromagnet Res Inst, Koganei, Tokyo 1848795, Japan.
   [Seto, Shinta] Nagasaki Univ, Grad Sch Engn, Nagasaki 8528521, Japan.
   [Meneghini, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Awaka, Jun] Tokai Univ, Liberal Arts Educ Ctr, Sapporo, Hokkaido 0058601, Japan.
RP Kubota, T (reprint author), Japan Aerosp Explorat Agcy, Earth Observat Res Ctr, Tsukuba, Ibaraki 3058505, Japan.
EM kubota.takuji@jaxa.jp
RI Kubota, Takuji/E-6024-2011; Measurement, Global/C-4698-2015; PMM,
   JAXA/K-8537-2016
OI Kubota, Takuji/0000-0003-0282-1075; 
NR 57
TC 9
Z9 9
U1 4
U2 21
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 2014
VL 7
IS 9
SI SI
BP 3931
EP 3944
DI 10.1109/JSTARS.2014.2320960
PG 14
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
   Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
   Photographic Technology
GA AT5ON
UT WOS:000344992200024
ER

PT J
AU Fok, MC
   Buzulukova, NY
   Chen, SH
   Glocer, A
   Nagai, T
   Valek, P
   Perez, JD
AF Fok, M. -C.
   Buzulukova, N. Y.
   Chen, S. -H.
   Glocer, A.
   Nagai, T.
   Valek, P.
   Perez, J. D.
TI The Comprehensive Inner Magnetosphere-Ionosphere Model
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID RADIATION BELT ELECTRONS; RING CURRENT DEVELOPMENT; RICE CONVECTION
   MODEL; PLASMA SHEET; GEOMAGNETIC STORMS; RELATIVISTIC ELECTRONS;
   ENERGETIC PARTICLE; CURRENT IONS; ACCELERATION; MISSION
AB Simulation studies of the Earth's radiation belts and ring current are very useful in understanding the acceleration, transport, and loss of energetic particles. Recently, the Comprehensive Ring Current Model (CRCM) and the Radiation Belt Environment (RBE) model were merged to form a Comprehensive Inner Magnetosphere-Ionosphere (CIMI) model. CIMI solves for many essential quantities in the inner magnetosphere, including ion and electron distributions in the ring current and radiation belts, plasmaspheric density, Region 2 currents, convection potential, and precipitation in the ionosphere. It incorporates whistler mode chorus and hiss wave diffusion of energetic electrons in energy, pitch angle, and cross terms. CIMI thus represents a comprehensive model that considers the effects of the ring current and plasmasphere on the radiation belts. We have performed a CIMI simulation for the storm on 5-9 April 2010 and then compared our results with data from the Two Wide-angle Imaging Neutral-atom Spectrometers and Akebono satellites. We identify the dominant energization and loss processes for the ring current and radiation belts. We find that the interactions with the whistler mode chorus waves are the main cause of the flux increase of MeV electrons during the recovery phase of this particular storm. When a self-consistent electric field from the CRCM is used, the enhancement of MeV electrons is higher than when an empirical convection model is applied. We also demonstrate how CIMI can be a powerful tool for analyzing and interpreting data from the new Van Allen Probes mission.
C1 [Fok, M. -C.; Buzulukova, N. Y.; Chen, S. -H.; Glocer, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Buzulukova, N. Y.] Univ Maryland, Ctr Res & Explorat Space Sci & Technol, College Pk, MD 20742 USA.
   [Chen, S. -H.] Univ Space Res Assoc, Ctr Res & Explorat Space Sci & Technol, Columbia, MD USA.
   [Nagai, T.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Tokyo 152, Japan.
   [Valek, P.] SW Res Inst, San Antonio, TX USA.
   [Perez, J. D.] Auburn Univ, Dept Phys, Auburn, AL 36849 USA.
RP Fok, MC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM mei-ching.h.fok@nasa.gov
OI Valek, Philip/0000-0002-2318-8750
FU TWINS mission as a part of NASA's Explorer Program; NASA Heliophysics
   Living With a Star Targeted Research and Technology program, under Work
   Breakdown Structure [936723.02.01.09.47]; Van Allen Probes mission
   funding
FX The authors thank Donald Fairfield for many valuable comments. We thank
   ACE, WIND, and OMNI teams for providing solar wind data through Space
   Physics Data Facility of NASA Goddard Space Flight Center. The AL, AU,
   Dst and SYM-H indices are provided by Kyoto University World Data Center
   for Geomagnetism. We also gratefully acknowledge Jay Albert of Air Force
   Research Laboratory for providing the VLF wave diffusion coefficients.
   The TWINS data shown in this paper were downloaded at the TWINS website
   at http://twins.swri.edu. To access the Akebono data, contact Tsugunobu
   Nagai at nagai@geo.titech.ac.jp. This work was supported by the TWINS
   mission as a part of NASA's Explorer Program, and by NASA Heliophysics
   Living With a Star Targeted Research and Technology program, under Work
   Breakdown Structure 936723.02.01.09.47. Part of the research in this
   paper was supported by Van Allen Probes mission funding.
NR 115
TC 12
Z9 12
U1 0
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2014
VL 119
IS 9
DI 10.1002/2014JA020239
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BN
UT WOS:000344810200035
ER

PT J
AU Kajdic, P
   Lavraud, B
   Zaslavsky, A
   Blanco-Cano, X
   Sauvaud, JA
   Opitz, A
   Jian, LK
   Maksimovic, M
   Luhmann, JG
AF Kajdic, P.
   Lavraud, B.
   Zaslavsky, A.
   Blanco-Cano, X.
   Sauvaud, J-A
   Opitz, A.
   Jian, L. K.
   Maksimovic, M.
   Luhmann, J. G.
TI Ninety degrees pitch angle enhancements of suprathermal electrons
   associated with interplanetary shocks
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SOLAR-WIND ELECTRONS; EARTHS BOW SHOCK; VELOCITY DISTRIBUTIONS; RADIAL
   EVOLUTION; GLOBAL PROCESSES; FIELD LINES; STEREO; PLASMA; IMPACT;
   DEPLETIONS
AB We report the results of the first systematic analysis of 90 degrees pitch angle (PA) enhancements or the ring distributions of suprathermal (E similar to 70 eV-2 keV) electrons at interplanetary (IP) shocks. We analyze 2 h time intervals around 232 IP shocks observed by the two STEREO spacecraft between 2007 and 2011. The ring distributions were detected downstream of 114 events (49%). In 52 (22.4%) cases they were detected at the shock ramp. We also found 90 degrees enhancements upstream of 11 (4.7%) events. Statistical analysis of basic shock properties did not reveal substantial differences between the shocks that are associated with the enhancements and those that are not. The data from the STEREO/WAVES instruments revealed that the 90 degrees PA enhancements tend to be associated with magnetic and electric field fluctuations. Although at this point we do not have a satisfactory explanation for the mechanism that produces these distributions, our findings suggest that wave-particle interactions play a role, while pure focusing and mirroring effects due to adiabatic motion of electrons across the shock fronts cannot fully account for the observations.
C1 [Kajdic, P.; Lavraud, B.; Sauvaud, J-A] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
   [Kajdic, P.; Lavraud, B.; Sauvaud, J-A] CNRS, IRAP, Toulouse, France.
   [Kajdic, P.; Opitz, A.] European Space Agcy, European Space Res & Technol Ctr, NL-2200 AG Noordwijk, Netherlands.
   [Zaslavsky, A.; Maksimovic, M.] Univ Paris 07, Univ Paris 06, CNRS, LESIA,Observ Paris, Paris, France.
   [Blanco-Cano, X.] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico.
   [Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Jian, L. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Kajdic, P (reprint author), Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
EM kajdic@gmail.com
RI Jian, Lan/B-4053-2010
OI Jian, Lan/0000-0002-6849-5527
FU CNRS; CNES; ESA research fellowship; NASA's Science Mission Directorate
   as part of the STEREO project
FX The authors acknowledge the CL/CLWeb team (http://clweb.cesr.fr). P.K.'s
   and A.O.'s work was possible due to an ESA research fellowship. The work
   at IRAP was supported by CNRS and CNES. L.K.J.'s and J.G.L.'s work is
   supported by NASA's Science Mission Directorate as part of the STEREO
   project, including the IMPACT and PLASTIC investigations. The French
   contribution to the S/WAVES investigation has been supported by both
   CNES and CNRS. X. B. C. is grateful for DGAPA grant PAPIIT IN105014. The
   authors also acknowledge Karim Meziane for useful discussions on
   Liouville mapping.
NR 53
TC 2
Z9 2
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2014
VL 119
IS 9
DI 10.1002/2014JA020213
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BN
UT WOS:000344810200004
ER

PT J
AU Kissinger, J
   Kepko, L
   Baker, DN
   Kanekal, S
   Li, W
   McPherron, RL
   Angelopoulos, V
AF Kissinger, Jennifer
   Kepko, Larry
   Baker, Daniel N.
   Kanekal, Shri
   Li, Wen
   McPherron, Robert L.
   Angelopoulos, Vassilis
TI The importance of storm time steady magnetospheric convection in
   determining the final relativistic electron flux level
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID OUTER RADIATION BELT; ENERGETIC PARTICLE INJECTIONS; INNER
   MAGNETOSPHERE; LOCAL ACCELERATION; MAGNETIC-FIELD; CHORUS; SUBSTORM;
   PRECIPITATION; SIMULATION; TRANSPORT
AB Relativistic electrons pose a space weather hazard to satellites in the radiation belts. Although about half of all geomagnetic storms result in relativistic electron flux enhancements, other storms decrease relativistic electron flux, even under similar solar wind drivers. Radiation belt fluxes depend on a complex balance between transport, loss, and acceleration. A critically important aspect of radiation belt enhancements is the role of the "seed" population-plasma sheet particles heated and transported earthward by magnetotail processes-which can become accelerated by wave-particle interactions with chorus waves. While the effect of substorms on seed electron injections has received considerable focus, in this study we present a previously unexplored connection between quasi-steady convection during steady magnetospheric convection (SMC) events and the transport and energization of electrons. SMC events are long-duration intervals of enhanced convection without any substorm expansions and are an important mechanism in coupling magnetotail plasma populations to the innermagnetosphere. We find that storms with SMCs in the recovery phase aremore likely to increase relativistic electron flux levels, while storms without SMCs aremore likely to result in a decrease. Using particle measurements from the Time History of Events and Macroscale Interactions During Substorms mission, we show that phase space density of seed electron populations increases 1 h before SMC start and stays elevated through the duration of SMCs. Chorus activity is also elevated during SMC events. These results suggest that rather than hindering electron acceleration by diverting plasma away from the inner magnetosphere, SMC events appear to act to enhance and maintain seed electron populations.
C1 [Kissinger, Jennifer; Kepko, Larry; Kanekal, Shri] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Baker, Daniel N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
   [Li, Wen] Univ Calif Los Angeles, Atmospher & Ocean Sci Dept, Los Angeles, CA USA.
   [McPherron, Robert L.; Angelopoulos, Vassilis] Univ Calif Los Angeles, Earth Planetary & Space Sci Dept, Los Angeles, CA USA.
RP Kissinger, J (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM jenni.kissinger@gmail.com
FU NASA
FX We would like to thank Drew Turner for help with calculating THEMIS
   phase space densities and Jacob Bortnik for helpful discussions on
   chorus-electron interactions. J. Kissinger 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 solar wind data and SYM-H index are available at
   1 min resolution through the OMNI data set at the Space Physics Data
   Facility's (SPDF) Coordinated Data Analysis Website
   (http://cdaweb.gsfc.nasa.gov/istp_public/). THEMIS particle and field
   data are similarly provided by CDAWeb or by downloading with the use of
   the TDAS IDL software. SAMPEX PET electron fluxes are also available
   from CDAWeb. The auroral indices AL and AU are available from the World
   Data Center for Geomagnetism in Kyoto, Japan
   (http://wdc.kugi.kyoto-u.ac.jp/) or as part of the OMNI data set.
NR 60
TC 3
Z9 3
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 2014
VL 119
IS 9
DI 10.1002/2014JA019948
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BN
UT WOS:000344810200029
ER

PT J
AU Muzamil, FM
   Farrugia, CJ
   Torbert, RB
   Pritchett, PR
   Mozer, FS
   Scudder, JD
   Russell, CT
   Sandholt, PE
   Denig, WF
   Wilson, L
AF Muzamil, F. M.
   Farrugia, C. J.
   Torbert, R. B.
   Pritchett, P. R.
   Mozer, F. S.
   Scudder, J. D.
   Russell, C. T.
   Sandholt, P. E.
   Denig, W. F.
   Wilson, L., III
TI Structure of a reconnection layer poleward of the cusp: Extreme density
   asymmetry and a guide field
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID INTERPLANETARY MAGNETIC-FIELD; EARTHS MAGNETOSPHERE; PLASMA INSTRUMENT;
   ELECTRIC-FIELD; CURRENT SHEET; SOLAR-WIND; POLAR-CAP; MAGNETOPAUSE;
   CONVECTION; COMPONENT
AB We present Polar observations of a reconnection layer during an inbound pass at high northern latitudes. The interplanetary field of 20 nT pointed strongly northward continuously for 13 h. Reverse polar cap convection observed repeatedly by the DMSP F13 satellite provided direct evidence of continued reconnection. Polar observed sunward and southward jets. The event was hallmarked by a density asymmetry approximate to 140 and moderate guide field. Disturbances in fields and plasma were much more intense on the magnetosphere (MSP) side of the current sheet (CS). A density cavity was observed at both separatrices. Isolated E-N peaks occurred at the density cavity regions. The intense electric field fluctuations (<= 60 mV/m) were mainly in the component normal to the CS, E-N. The guide field pointed opposite to the Hall field, leading to an overall weakening of the out-of-plane magnetic field. A magnetic island was observed in the outflow jet. The field reversal at the CS occurred before the outflow jet, which we argue to be due to the large density asymmetry. The stagnation line was strongly shifted toward the MSP side of the CS. We compare observations with simulations which emphasize the density asymmetry and which also include a guide field, and we find good agreement. Remaining discrepancies may be explained by a density asymmetry much larger than in simulations. This is to our knowledge the first study of a high-latitude reconnection layer with (1) an extreme density asymmetry and (2) steady and continuously strong interplanetary B-z.
C1 [Muzamil, F. M.; Farrugia, C. J.; Torbert, R. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
   [Pritchett, P. R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA.
   [Mozer, F. S.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
   [Mozer, F. S.] Univ Calif Berkeley, Space Sci Labs, Berkeley, CA 94720 USA.
   [Scudder, J. D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
   [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
   [Sandholt, P. E.] Univ Oslo, Dept Phys, Oslo, Norway.
   [Denig, W. F.] NOAA, Natl Geophys Data Ctr, Boulder, CO 80303 USA.
   [Wilson, L., III] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Farrugia, CJ (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
EM charlie.farrugia@unh.edu
RI Wilson III, Lynn/D-4425-2012
OI Wilson III, Lynn/0000-0002-4313-1970
FU NASA [NNX09AE41G-1/14, NNX13AP39G]; NASA/WIND [NNX10AQA29G]
FX This work was supported by NASA grants NNX09AE41G-1/14 and NNX13AP39G
   and NASA/WIND grant NNX10AQA29G.
NR 68
TC 4
Z9 4
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2014
VL 119
IS 9
DI 10.1002/2014JA019879
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BN
UT WOS:000344810200024
ER

PT J
AU Randol, BM
   Christian, ER
AF Randol, Brent M.
   Christian, Eric R.
TI Simulations of plasma obeying Coulomb's law and the formation of
   suprathermal ion tails in the solar wind
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID VELOCITY DISTRIBUTIONS; COMPUTER-SIMULATION; KAPPA-DISTRIBUTIONS;
   TERMINATION SHOCK; ACCELERATION; EQUILIBRIUM; HELIOSPHERE; VARIABILITY;
   ELECTRONS; ENERGIES
AB We present a model for the velocity distribution function (VDF) of the suprathermal ion tail in the solar wind and its commonly observed spectrum, a power law in velocity of index -5. The mechanism for our model is acceleration from extremely small scale electric fields caused by the finite number of particles in the solar wind (or any plasma). The simulations produce a VDF with a broken power law at short times and a type of.. distribution VDF at later times. The simulation uses very few assumptions as it is based solely on Coulomb's law, and the results are robust to a range of parameters that, although outside the range of the solar wind at 1 AU, are close to those in the lower solar atmosphere. Furthermore, we provide predictions based on the following mechanism: the probability distribution function for the electric field (the electric field distribution function or EDF) dictates the final state of the plasma, which means that the VDF at any time is a convolution of the initial VDF and the EDF. We have also shown that by varying the power law index of the electrostatic force law, the relationship between the two is such that the EDF power law index is exactly 5 for Coulomb's law, harder for shorter-range forces, and softer for longer-range forces, converging to a power law of index 3 in the former limit and to a Maxwellian in the latter.
C1 [Randol, Brent M.; Christian, Eric R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Randol, BM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM brent.m.randol@nasa.gov
FU NASA
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. As per AGU's Data
   Policy, the corresponding author may be contacted in order to access any
   relevant data related to this article.
NR 50
TC 5
Z9 5
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2014
VL 119
IS 9
DI 10.1002/2014JA020095
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BN
UT WOS:000344810200003
ER

PT J
AU Sitnov, MI
   Merkin, VG
   Swisdak, M
   Motoba, T
   Buzulukova, N
   Moore, TE
   Mauk, BH
   Ohtani, S
AF Sitnov, M. I.
   Merkin, V. G.
   Swisdak, M.
   Motoba, T.
   Buzulukova, N.
   Moore, T. E.
   Mauk, B. H.
   Ohtani, S.
TI Magnetic reconnection, buoyancy, and flapping motions in magnetotail
   explosions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID HYBRID-DRIFT INSTABILITY; PLASMA SHEET; EARTHS MAGNETOTAIL; NEUTRAL
   SHEET; GROWTH-PHASE; STATISTICAL VISUALIZATION; ENERGY-CONVERSION;
   STELLAR FLARES; FLUX TUBES; SIMULATIONS
AB A key process in the interaction of magnetospheres with the solar wind is the explosive release of energy stored in the magnetotail. Based on observational evidence, magnetic reconnection is widely believed to be responsible. However, the very possibility of spontaneous reconnection in collisionless magnetotail plasmas has been questioned in kinetic theory for more than three decades. In addition, in situ observations by multispacecraft missions (e. g., THEMIS) reveal the development of buoyancy and flapping motions coexisting with reconnection. Never before have kinetic simulations reproduced all three primary modes in realistic 2-D configurations with a finite normal magnetic field. Moreover, 3-D simulations with closed boundaries suggest that the tail activity is dominated by buoyancy-driven instabilities, whereas reconnection is a secondary effect strongly localized in the dawn-dusk direction. In this paper, we use massively parallel 3-D fully kinetic simulations with open boundaries to show that sufficiently far from the planet explosive processes in the tail are dominated by reconnection motions. These motions occur in the form of spontaneously generated dipolarization fronts accompanied by changes in magnetic topology which extend in the dawn-dusk direction over the size of the simulation box, suggesting that reconnection onset causes a macroscale reconfiguration of the real magnetotail. In our simulations, buoyancy and flapping motions significantly disturb the primary dipolarization front but neither destroy it nor change the near 2-D picture of the front evolution critically. Consistent with recent multiprobe observations, dipolarization fronts are also found to be the main regions of energy conversion in the magnetotail.
C1 [Sitnov, M. I.; Merkin, V. G.; Motoba, T.; Mauk, B. H.; Ohtani, S.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
   [Swisdak, M.] Univ Maryland, Inst Res Elect & Appl Phys, College Pk, MD 20742 USA.
   [Buzulukova, N.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Buzulukova, N.; Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sitnov, MI (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
EM Mikhail.Sitnov@jhuapl.edu
RI Merkin, Viacheslav/D-5982-2016; Ohtani, Shinichi/E-3914-2016; Sitnov,
   Mikhail/H-2316-2016; Mauk, Barry/E-8420-2017
OI Merkin, Viacheslav/0000-0003-4344-5424; Ohtani,
   Shinichi/0000-0002-9565-6840; Mauk, Barry/0000-0001-9789-3797
FU NASA [NNX12AD31G, NNX13AD66G, NNX13AF82G]; NSF [AGS1403144]; NASA
   Magnetospheric Multiscale Mission
FX The authors thank P.C. Brandt, J.C. Dorelli, D.-Y. Lee, E.V. Panov, and
   P.L. Pritchett for useful discussions. This work was supported by NASA
   grants NNX12AD31G, NNX13AD66G, and NNX13AF82G as well as NSF grant
   AGS1403144. The contribution of NB and TEM was supported by the NASA
   Magnetospheric Multiscale Mission. Simulations were made possible by the
   NASA High-End Computing (HEC) Program through the NASA Advanced
   Supercomputing (NAS) Division at Ames Research Center. The authors would
   like to acknowledge the support of the NAS personnel and especially
   Johnny Chang for their help with the job optimization. The data used to
   produce figures, animations, and analysis in the paper are available
   upon request.
NR 99
TC 22
Z9 22
U1 0
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 2014
VL 119
IS 9
DI 10.1002/2014JA020205
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BN
UT WOS:000344810200012
ER

PT J
AU Wang, X
   Malaspina, DM
   Hsu, HW
   Ergun, RE
   Horanyi, M
AF Wang, X.
   Malaspina, D. M.
   Hsu, H-W
   Ergun, R. E.
   Horanyi, M.
TI The effects of magnetic fields on photoelectron-mediated spacecraft
   potential fluctuations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID DENSITIES; ESCAPE
AB Previously, we have experimentally studied photoelectron-mediated spacecraft potential fluctuations associated with time-dependent external electric fields. In this paper, we investigate the effects of magnetic fields on such spacecraft potential fluctuations. A magnetic field is created above the UV-illuminated surface of a spacecraft model to alter the escape rate of photoelectrons. The packet of the observed potential oscillations becomes less positive with increasing magnetic field strength because more of the emitted photoelectrons are returned to the surface. As a result, the photoelectric charging time is increased, corresponding to a decrease in the response frequency of the photoemitting surface. The amplitude of the potential oscillations decreases when the response frequency becomes lower than the electric field oscillation frequency. A test particle simulation is validated with the laboratory experiments and applied to estimate the photoelectron escape rate from the Van Allen Probes spacecraft, showing that the photoelectron current is reduced by as much as 30% when magnetic field strength is 1200 nT. Based on our laboratory results and computer simulations, we discuss the effects of magnetic fields on the spacecraft potential fluctuations observed by the Van Allen Probes.
C1 [Wang, X.; Malaspina, D. M.; Hsu, H-W; Ergun, R. E.; Horanyi, M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
   [Wang, X.; Hsu, H-W; Horanyi, M.] NASA, SSERVIs, Inst Modeling Plasma Atmospheres & Cosm Dust, Boulder, CO USA.
RP Wang, X (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
EM xu.wang@colorado.edu
FU NASA's Van Allen Probes program [NAS5-01072]; NASA/SSERVI's Institute
   for Modeling Plasma, Atmospheres, and Cosmic Dust (IMPACT)
FX This work was supported by the NASA's Van Allen Probes program (award
   NAS5-01072) and by the NASA/SSERVI's Institute for Modeling Plasma,
   Atmospheres, and Cosmic Dust (IMPACT). The experimental data for this
   paper are available on request.
NR 13
TC 0
Z9 0
U1 2
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 2014
VL 119
IS 9
DI 10.1002/2014JA019923
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AT3BN
UT WOS:000344810200022
ER

PT J
AU Teixeira, J
   Waliser, D
   Ferraro, R
   Gleckler, P
   Lee, T
   Potter, G
AF Teixeira, Joao
   Waliser, Duane
   Ferraro, Robert
   Gleckler, Peter
   Lee, Tsengdar
   Potter, Gerald
TI Satellite Observations for CMIP5 The Genesis of Obs4MIPs
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Editorial Material
C1 [Teixeira, Joao; Waliser, Duane; Ferraro, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Gleckler, Peter] Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA USA.
   [Lee, Tsengdar] NASA HQ, Washington, DC USA.
   [Potter, Gerald] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Teixeira, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM joao.teixeira@jpl.nasa.gov
NR 8
TC 17
Z9 17
U1 0
U2 5
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 2014
VL 95
IS 9
BP 1329
EP 1334
DI 10.1175/BAMS-D-12-00204.1
PG 6
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS7MY
UT WOS:000344441200007
ER

PT J
AU Rosenzweig, C
   Horton, RM
   Bader, DA
   Brown, ME
   DeYoung, R
   Dominguez, O
   Fellows, M
   Friedl, L
   Graham, W
   Hall, C
   Higuchi, S
   Iraci, L
   Jedlovec, G
   Kaye, J
   Loewenstein, M
   Mace, T
   Milesi, C
   Patzert, W
   Stackhouse, PW
   Toufectis, K
AF Rosenzweig, Cynthia
   Horton, Radley M.
   Bader, Daniel A.
   Brown, Molly E.
   DeYoung, Russell
   Dominguez, Olga
   Fellows, Merrilee
   Friedl, Lawrence
   Graham, William
   Hall, Carlton
   Higuchi, Sam
   Iraci, Laura
   Jedlovec, Gary
   Kaye, Jack
   Loewenstein, Max
   Mace, Thomas
   Milesi, Cristina
   Patzert, William
   Stackhouse, Paul W., Jr.
   Toufectis, Kim
TI ENHANCING CLIMATE RESILIENCE AT NASA CENTERS A Collaboration between
   Science and Stewardship
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID SEA-LEVEL RISE; WEST ANTARCTICA; ICE SHEETS; PROJECTIONS; SCENARIOS;
   THWAITES; IMPACTS; COAST
C1 [Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
   [Rosenzweig, Cynthia; Horton, Radley M.; Bader, Daniel A.] Columbia Univ, Earth Inst, Ctr Climate Syst Res, New York, NY USA.
   [Brown, Molly E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [DeYoung, Russell; Stackhouse, Paul W., Jr.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
   [Dominguez, Olga; Fellows, Merrilee; Friedl, Lawrence; Higuchi, Sam; Kaye, Jack; Toufectis, Kim] NASA Headquarters, Washington, DC USA.
   [Graham, William] NASA, Stennis Space Ctr, Mississippi State, MS USA.
   [Hall, Carlton] NASA, Kennedy Space Ctr, InoMed Hlth Applicat Inc, Orlando, FL USA.
   [Iraci, Laura; Loewenstein, Max; Milesi, Cristina] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Jedlovec, Gary] NASA, Marshall Space Flight Ctr, Huntsville, AL USA.
   [Mace, Thomas] NASA, Dryden Flight Res Ctr, Edwards AFB, CA USA.
   [Milesi, Cristina] Calif State Univ Monterey Bay, Seaside, CA USA.
   [Patzert, William] NASA, Jet Prop Lab, Pasadena, CA USA.
RP Rosenzweig, C (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM cynthia.rosenzweig@nasa.gov
RI Brown, Molly/E-2724-2010
OI Brown, Molly/0000-0001-7384-3314
FU NASA's Earth Science Division and Applied Sciences Program; National
   Science Foundation (NSF); U.S. DOE; NOAA; U.S. Environmental Protection
   Agency Office of Research and Development
FX CASI is supported by NASA's Earth Science Division and Applied Sciences
   Program.; We also thank the North American Regional Climate Change
   Assessment Program (NARCCAP) for providing data. NARCCAP is funded by
   the National Science Foundation (NSF), the U.S. DOE, NOAA, and the U.S.
   Environmental Protection Agency Office of Research and Development.
NR 59
TC 4
Z9 4
U1 2
U2 5
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 2014
VL 95
IS 9
BP 1351
EP 1363
DI 10.1175/BAMS-D-12-00169.1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS7MY
UT WOS:000344441200010
ER

PT J
AU Machado, LAT
   Dias, MAFS
   Morales, C
   Fisch, G
   Vila, D
   Albrecht, R
   Goodman, SJ
   Calheiros, AJP
   Biscaro, T
   Kummerow, C
   Cohen, J
   Fitzjarrald, D
   Nascimento, EL
   Sakamoto, MS
   Cunningham, C
   Chaboureau, JP
   Petersen, WA
   Adams, DK
   Baldini, L
   Angelis, CF
   Sapucci, LF
   Salio, P
   Barbosa, HMJ
   Landulfo, E
   Souza, RAF
   Blakeslee, RJ
   Bailey, J
   Freitas, S
   Lima, WFA
   Tokay, A
AF Machado, Luiz A. T.
   Silva Dias, Maria A. F.
   Morales, Carlos
   Fisch, Gilberto
   Vila, Daniel
   Albrecht, Rachel
   Goodman, Steven J.
   Calheiros, Alan J. P.
   Biscaro, Thiago
   Kummerow, Christian
   Cohen, Julia
   Fitzjarrald, David
   Nascimento, Ernani L.
   Sakamoto, Meiry S.
   Cunningham, Christopher
   Chaboureau, Jean-Pierre
   Petersen, Walter A.
   Adams, David K.
   Baldini, Luca
   Angelis, Carlos F.
   Sapucci, Luiz F.
   Salio, Paola
   Barbosa, Henrique M. J.
   Landulfo, Eduardo
   Souza, Rodrigo A. F.
   Blakeslee, Richard J.
   Bailey, Jeffrey
   Freitas, Saulo
   Lima, Wagner F. A.
   Tokay, Ali
TI THE CHUVA PROJECT How Does Convection Vary across Brazil?
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID SIZE DISTRIBUTIONS; CLOUD CLUSTERS; SOUTH-AMERICA; WEATHER RADAR; SQUALL
   LINES; WARM-RAIN; SATELLITE; PRECIPITATION; TROPICS; THUNDERSTORMS
C1 [Machado, Luiz A. T.; Vila, Daniel; Albrecht, Rachel; Calheiros, Alan J. P.; Biscaro, Thiago; Cunningham, Christopher; Angelis, Carlos F.; Sapucci, Luiz F.; Freitas, Saulo; Lima, Wagner F. A.] Inst Nacl Pesquisas Espacials, Ctr Previsao Tempo & Estudos Climat, Sao Jose Dos Campos, Brazil.
   [Silva Dias, Maria A. F.; Morales, Carlos] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Sao Paulo, Brazil.
   [Fisch, Gilberto] Inst Aeronaut & Espaco, Dept Ciencia & Tecnol Aeroespacial, Sao Paulo, Brazil.
   [Goodman, Steven J.] GSFC, Greenbelt, MD USA.
   [Kummerow, Christian] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
   [Cohen, Julia] Fed Univ Para, Inst Geociencias, BR-66059 Belem, Para, Brazil.
   [Fitzjarrald, David] SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12222 USA.
   [Nascimento, Ernani L.] Univ Fed Santa Maria, Dept Fis, BR-97119900 Santa Maria, RS, Brazil.
   [Sakamoto, Meiry S.] Fundacao Cearense Meteorol, Fortaleza, Ceara, Brazil.
   [Chaboureau, Jean-Pierre] Univ Toulouse, Lab Aerol, Toulouse, France.
   [Petersen, Walter A.] NASA Wallops Flight Facil, Wallops Isl, VA USA.
   [Adams, David K.] Univ Nacl Autonoma Mexico, Ctr Ciencias Atmosfera, Mexico City 04510, DF, Mexico.
   [Baldini, Luca] CNR, Ist Sci Atmosfera & Clima, Rome, Italy.
   [Salio, Paola] Univ Buenos Aires, Buenos Aires, DF, Argentina.
   [Barbosa, Henrique M. J.] Univ Sao Paulo, Inst Fis, BR-01498 Sao Paulo, Brazil.
   [Landulfo, Eduardo] Inst Pesquisas Energet & Nucl, Sao Paulo, Brazil.
   [Souza, Rodrigo A. F.] Univ Estado Amazonas, Manaus, Amazonas, Brazil.
   [Blakeslee, Richard J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
   [Bailey, Jeffrey] Univ Alabama, Huntsville, AL 35899 USA.
   [Tokay, Ali] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
RP Machado, LAT (reprint author), Inst Nacl Pesquisas Espacials, Ctr Previsao Tempo & Estudos Climat, Rodovia Pres Dutra,Km 40, BR-12630000 Cachoeira Paulista, SP, Brazil.
EM luiz.machado@cptec.inpe.br
RI Sapucci, Luiz/B-2345-2014; Freitas, Saulo/A-2279-2012; Barbosa,
   Henrique/F-3499-2012; Vila, Daniel/G-8379-2012; Nesbitt,
   Stephen/I-3965-2013; Landulfo, Eduardo/B-7979-2012; Measurement,
   Global/C-4698-2015; 
OI Freitas, Saulo/0000-0002-9879-646X; Barbosa,
   Henrique/0000-0002-4027-1855; Vila, Daniel/0000-0002-1015-5650; Nesbitt,
   Stephen/0000-0003-0348-0452; Landulfo, Eduardo/0000-0002-9691-5306;
   Baldini, Luca/0000-0001-5217-1205
FU FAPESP [2009/15235-8]
FX This work was supported by FAPESP Grant 2009/15235-8, the CHUVA Project.
   Special thanks to Mario Figueiredo for maintaining the CHUVA database;
   Claudinei Camargo for assisting in figure preparation; Jorge Melo and
   Jorge Marton for their engineering support during the field campaigns;
   Moacir Lacerda, Evandro Anselmo, and Joao Neves for their support during
   lightning installation; and Izabelly Carvalho for processing the
   disdrometer dataset. The authors acknowledge the anonymous reviewers and
   the comments provided by Earle Williams. The authors also thank all of
   the participants in the CHUVA field campaigns who contributed directly
   or indirectly during the years of field work.
NR 43
TC 25
Z9 25
U1 1
U2 17
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 2014
VL 95
IS 9
BP 1365
EP 1380
DI 10.1175/BAMS-D-13-00084.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA AS7MY
UT WOS:000344441200011
ER

PT J
AU Pankratius, V
   Mattmann, C
AF Pankratius, Victor
   Mattmann, Chris
TI COMPUTING IN ASTRONOMY: TO SEE THE UNSEEN
SO COMPUTER
LA English
DT Editorial Material
AB Advances in computing have empowered astronomers to explore the universe in greater detail. Software-defined instruments relying on digital data capture and processing are more powerful than ever and continue to bring us new knowledge about the universe and our place in it.
C1 [Pankratius, Victor] MIT, Haystack Observ, Cambridge, MA 02139 USA.
   [Mattmann, Chris] NASA, Jet Prop Lab, Pasadena, CA USA.
   [Mattmann, Chris] Univ So Calif, Los Angeles, CA 90089 USA.
RP Pankratius, V (reprint author), MIT, Haystack Observ, Cambridge, MA 02139 USA.
EM pankrat@mit.edu; mattmann@jpl.nasa.gov
NR 3
TC 1
Z9 1
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0018-9162
EI 1558-0814
J9 COMPUTER
JI Computer
PD SEP
PY 2014
VL 47
IS 9
BP 23
EP 25
PG 3
WC Computer Science, Hardware & Architecture; Computer Science, Software
   Engineering
SC Computer Science
GA AS8CO
UT WOS:000344478100017
ER

PT J
AU De Jong, EM
AF De Jong, Eric M.
TI Visualizing Big Data in Astronomy: The Automated Movie Production
   Environment Distribution and Display (AMPED) Pipeline
SO COMPUTER
LA English
DT Article
AB Storing, transporting, analyzing, and visualizing rapidly growing quantities of data is a significant challenge in astronomy. The Automated Movie Production Environment Distribution and Display (AMPED) Pipeline aims to enhance dataset usage through "movie" visualization.
C1 NASA Jet Prop Lab, Pasadena, CA 91109 USA.
RP De Jong, EM (reprint author), NASA Jet Prop Lab, Pasadena, CA 91109 USA.
EM Eric.M.DeJong@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This work was carried out at the Jet Propulsion Laboratory, California
   Institute of Technology, under contract with the National Aeronautics
   and Space Administration.
NR 0
TC 0
Z9 0
U1 0
U2 2
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0018-9162
EI 1558-0814
J9 COMPUTER
JI Computer
PD SEP
PY 2014
VL 47
IS 9
BP 64
EP 65
PG 2
WC Computer Science, Hardware & Architecture; Computer Science, Software
   Engineering
SC Computer Science
GA AS8CO
UT WOS:000344478100024
ER

PT J
AU Hart, AF
   Cinquini, L
   Khudikyan, SE
   Thompson, DR
   Mattmann, CA
   Wagstaff, K
   Lazio, J
   Jones, DL
AF Hart, Andrew F.
   Cinquini, Luca
   Khudikyan, Shakeh E.
   Thompson, David R.
   Mattmann, Chris A.
   Wagstaff, Kiri
   Lazio, Joseph
   Jones, Dayton L.
TI Supporting Distributed, Collaborative Review and Classification of Fast
   Transient Events
SO COMPUTER
LA English
DT Article
AB Open source software and machine learning help support a modern, high-throughput radio-astronomy experiment investigating fast transient events.
C1 [Hart, Andrew F.; Cinquini, Luca; Khudikyan, Shakeh E.; Thompson, David R.; Wagstaff, Kiri; Lazio, Joseph; Jones, Dayton L.] NASA Jet Prop Lab, Pasadena, CA 91109 USA.
   [Mattmann, Chris A.] NASA Jet Prop Lab, Instrument & Sci Data Syst Grp, Pasadena, CA USA.
RP Hart, AF (reprint author), NASA Jet Prop Lab, Pasadena, CA 91109 USA.
EM ahart@apache.org; Luca.cinquini@jpl.nasa.gov;
   Shakeh.e.khudikyan@jpl.nasa.gov; david.r.thompson@jpl.nasa.gov;
   mattmann@jpl.nasa.gov; Kiri.wagstaff@jpl.nasa.gov;
   Joseph.lazio@jpl.nasa.gov; Djones@jpl.nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0018-9162
EI 1558-0814
J9 COMPUTER
JI Computer
PD SEP
PY 2014
VL 47
IS 9
BP 65
EP 66
PG 2
WC Computer Science, Hardware & Architecture; Computer Science, Software
   Engineering
SC Computer Science
GA AS8CO
UT WOS:000344478100025
ER

PT J
AU Jones, DL
AF Jones, Dayton L.
TI Big Data Technologies at JPL
SO COMPUTER
LA English
DT Article
AB The author summarizes recent work at the Jet Propulsion Laboratory in four technology areas needed for solving big data challenges: low-power signal processing, real-time analysis using machine learning algorithms, scalable data archiving, and mining and data visualization. While the needs of future large radio-astronomy arrays motived much of this work, the same challenges appear in a wide range of research fields and industries.
C1 NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jones, DL (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Djones@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This work was carried out at the Jet Propulsion Laboratory, California
   Institute of Technology, under contract with the National Aeronautics
   and Space Administration.
NR 0
TC 0
Z9 0
U1 0
U2 4
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0018-9162
EI 1558-0814
J9 COMPUTER
JI Computer
PD SEP
PY 2014
VL 47
IS 9
BP 67
EP 68
PG 2
WC Computer Science, Hardware & Architecture; Computer Science, Software
   Engineering
SC Computer Science
GA AS8CO
UT WOS:000344478100026
ER

PT J
AU Yang, GW
   Person, S
   Rungta, N
   Khurshid, S
AF Yang, Guowei
   Person, Suzette
   Rungta, Neha
   Khurshid, Sarfraz
TI Directed Incremental Symbolic Execution
SO ACM TRANSACTIONS ON SOFTWARE ENGINEERING AND METHODOLOGY
LA English
DT Article
DE Verification; Algorithms; Program differencing; symbolic execution;
   software evolution
ID SYSTEMS
AB The last few years have seen a resurgence of interest in the use of symbolic execution-a program analysis technique developed more than three decades ago to analyze program execution paths. Scaling symbolic execution to real systems remains challenging despite recent algorithmic and technological advances. An effective approach to address scalability is to reduce the scope of the analysis. For example, in regression analysis, differences between two related program versions are used to guide the analysis. While such an approach is intuitive, finding efficient and precise ways to identify program differences, and characterize their impact on how the program executes has proved challenging in practice.
   In this article, we present Directed Incremental Symbolic Execution (DiSE), a novel technique for detecting and characterizing the impact of program changes to scale symbolic execution. The novelty of DiSE is to combine the efficiencies of static analysis techniques to compute program difference information with the precision of symbolic execution to explore program execution paths and generate path conditions affected by the differences. DiSE complements other reduction and bounding techniques for improving symbolic execution. Furthermore, DiSE does not require analysis results to be carried forward as the software evolves-only the source code for two related program versions is required. An experimental evaluation using our implementation of DiSE illustrates its effectiveness at detecting and characterizing the effects of program changes.
C1 [Yang, Guowei] Texas State Univ, Dept Comp Sci, San Marcos, TX 78666 USA.
   [Person, Suzette] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
   [Rungta, Neha] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Khurshid, Sarfraz] Univ Texas Austin, Dept Elect & Comp Engn, Austin, TX 78712 USA.
RP Yang, GW (reprint author), Texas State Univ, Dept Comp Sci, San Marcos, TX 78666 USA.
EM GYang@txstate.edu
FU NSF [IIS-0438967, CCF-0845628, CCF-1319688, CNS-0958231]; AFOSR
   [FA9550-09-1-0351]
FX The work of G. Yang and S. Khurshid was supported in part by the NSF
   under Grant Nos. IIS-0438967, CCF-0845628, CCF-1319688, and CNS-0958231,
   and AFOSR grant FA9550-09-1-0351.
NR 49
TC 0
Z9 0
U1 0
U2 1
PU ASSOC COMPUTING MACHINERY
PI NEW YORK
PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA
SN 1049-331X
EI 1557-7392
J9 ACM T SOFTW ENG METH
JI ACM Trans. Softw. Eng. Methodol.
PD SEP
PY 2014
VL 24
IS 1
AR 3
DI 10.1145/2629536
PG 42
WC Computer Science, Software Engineering
SC Computer Science
GA AS5OP
UT WOS:000344320200003
ER

PT J
AU Moore, CW
   Nimbarte, AD
   Rajulu, S
AF Moore, Christopher W.
   Nimbarte, Ashish D.
   Rajulu, Sudhakar
TI Kinematic compatibility between the body and a mock spacesuit during
   basic upper body motions
SO INTERNATIONAL JOURNAL OF INDUSTRIAL ERGONOMICS
LA English
DT Article
DE Kinematics; Dynamic modeling; Range of motion; Mock spacesuit; Upper
   body motions
ID INJURIES
AB In this study, a novel conceptual method was tested to study the kinematic mismatch between the body motion of an occupant with respect to a rigid suit. It was hypothesized that differences between body and suit motion would require extra body movement to achieve the desired suit motion. To quantify the mismatch in kinematics, mock upper body suits with an open structure were used in conjunction with a marker-based motion capture system. A 3D motion modeling software was used to determine the range of motion of the suit and body segments of nine participants performing seven basic arm and trunk motions. In general, range of motion of the body segment was found to be higher than the corresponding suit segment range of motion. Differences in range of motion of up to 21.3% were found between corresponding body and suit segments, and significance was found in five of the seven motions. Relevance to industry: Development of a method of determining kinematic misalignment of protective suits will assist evaluation and development of more appropriate protective suits. Better kinematic alignment will not only reduce the risk of injury, but can also improve comfort and benefit performance. (C) 2014 Elsevier B.V. All rights reserved.
C1 [Moore, Christopher W.; Nimbarte, Ashish D.] W Virginia Univ, Ind & Management Syst Engn, Morgantown, WV 26506 USA.
   [Rajulu, Sudhakar] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
RP Nimbarte, AD (reprint author), W Virginia Univ, Ind & Management Syst Engn, POB 6070, Morgantown, WV 26506 USA.
EM cmoore18@mix.wvu.edu; Ashish.Nimbarte@mail.wvu.edu;
   sudhakar.rajulu-1@nasa.gov
NR 13
TC 1
Z9 1
U1 2
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-8141
EI 1872-8219
J9 INT J IND ERGONOM
JI Int. J. Ind. Ergon.
PD SEP
PY 2014
VL 44
IS 5
BP 739
EP 746
DI 10.1016/j.ergon.2014.06.003
PG 8
WC Engineering, Industrial; Ergonomics
SC Engineering
GA AS7MH
UT WOS:000344439600016
ER

PT J
AU Harri, AM
   Genzer, M
   Kemppinen, O
   Gomez-Elvira, J
   Haberle, R
   Polkko, J
   Savijarvi, H
   Renno, N
   Rodriguez-Manfredi, JA
   Schmidt, W
   Richardson, M
   Siili, T
   Paton, M
   Torre-Juarez, MD
   Makinen, T
   Newman, C
   Rafkin, S
   Mischna, M
   Merikallio, S
   Haukka, H
   Martin-Torres, J
   Komu, M
   Zorzano, MP
   Peinado, V
   Vazquez, L
   Urqui, R
AF Harri, A. -M.
   Genzer, M.
   Kemppinen, O.
   Gomez-Elvira, J.
   Haberle, R.
   Polkko, J.
   Savijaervi, H.
   Renno, N.
   Rodriguez-Manfredi, J. A.
   Schmidt, W.
   Richardson, M.
   Siili, T.
   Paton, M.
   Torre-Juarez, M. De La
   Maekinen, T.
   Newman, C.
   Rafkin, S.
   Mischna, M.
   Merikallio, S.
   Haukka, H.
   Martin-Torres, J.
   Komu, M.
   Zorzano, M. -P.
   Peinado, V.
   Vazquez, L.
   Urqui, R.
TI Mars Science Laboratory relative humidity observations: Initial results
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars; atmosphere; humidity; total water content; MSL; Gale
ID GENERAL-CIRCULATION MODEL; THERMAL EMISSION SPECTROMETER; MARTIAN
   ATMOSPHERE; WATER CYCLE; BOUNDARY-LAYER; SURFACE; SIMULATIONS; ROVER;
   ICE; PATHFINDER
AB The Mars Science Laboratory (MSL) made a successful landing at Gale crater early August 2012. MSL has an environmental instrument package called the Rover Environmental Monitoring Station (REMS) as a part of its scientific payload. REMS comprises instrumentation for the observation of atmospheric pressure, temperature of the air, ground temperature, wind speed and direction, relative humidity (REMS-H), and UV measurements. We concentrate on describing the REMS-H measurement performance and initial observations during the first 100 MSL sols as well as constraining the REMS-H results by comparing them with earlier observations and modeling results. The REMS-H device is based on polymeric capacitive humidity sensors developed by Vaisala Inc., and it makes use of transducer electronics section placed in the vicinity of the three humidity sensor heads. The humidity device is mounted on the REMS boom providing ventilation with the ambient atmosphere through a filter protecting the device from airborne dust. The final relative humidity results appear to be convincing and are aligned with earlier indirect observations of the total atmospheric precipitable water content. The water mixing ratio in the atmospheric surface layer appears to vary between 30 and 75 ppm. When assuming uniform mixing, the precipitable water content of the atmosphere is ranging from a few to six precipitable micrometers.
C1 [Harri, A. -M.; Genzer, M.; Kemppinen, O.; Polkko, J.; Savijaervi, H.; Schmidt, W.; Siili, T.; Paton, M.; Maekinen, T.; Merikallio, S.; Haukka, H.; Komu, M.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
   [Gomez-Elvira, J.; Rodriguez-Manfredi, J. A.; Martin-Torres, J.; Zorzano, M. -P.; Peinado, V.; Urqui, R.] Centro Astrobiol, Madrid, Spain.
   [Haberle, R.] NASA, Ames Res Ctr, San Francisco, CA USA.
   [Renno, N.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
   [Richardson, M.; Newman, C.] Ashima Res Inc, Pasadena, CA USA.
   [Torre-Juarez, M. De La; Mischna, M.] NASA, Jet Prop Lab, Pasadena, CA USA.
   [Rafkin, S.] Southwest Res Inst, Boulder, CO USA.
   [Vazquez, L.] Univ Complutense Madrid, Dept Appl Math, Madrid, Spain.
RP Harri, AM (reprint author), Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
EM Ari-Matti.Harri@fmi.fi
RI Rodriguez-Manfredi, Jose/L-8001-2014; Harri, Ari-Matti/C-7142-2012;
   Zorzano, Maria-Paz/F-2184-2015; Merikallio, Sini/C-7812-2014; Zorzano,
   Maria-Paz/C-5784-2015; Martin-Torres, Francisco Javier/G-6329-2015
OI Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Harri,
   Ari-Matti/0000-0001-8541-2802; Zorzano, Maria-Paz/0000-0002-4492-9650;
   Vazquez, Luis/0000-0003-4054-1197; Merikallio, Sini/0000-0001-7120-6127;
   Zorzano, Maria-Paz/0000-0002-4492-9650; Martin-Torres, Francisco
   Javier/0000-0001-6479-2236
FU Finnish Academy [132825, 131723]
FX The authors would like to express their gratitude to the MSL and REMS
   instrument teams in making this wonderful Mars mission come true.
   Ari-Matti Harri and Hannu Savijarvi are thankful for the Finnish Academy
   grants 132825 and 131723.
NR 48
TC 15
Z9 15
U1 0
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD SEP
PY 2014
VL 119
IS 9
BP 2132
EP 2147
DI 10.1002/2013JE004514
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AR8JH
UT WOS:000343820900007
ER

PT J
AU Shotwell, SK
   Hanselman, DH
   Belkin, IM
AF Shotwell, S. Kalei
   Hanselman, Dana H.
   Belkin, Igor M.
TI Toward biophysical synergy: Investigating advection along the Polar
   Front to identify factors influencing Alaska sablefish recruitment
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE Polar Front; Oceanic front; Sablefish; Groundfish; Stock assessment;
   Prediction; Modeling; Recruitment; Advection; Sea surface temperature;
   Gulf of Alaska; Alaska; North Pacific
ID CALIFORNIA CURRENT SYSTEM; STOCK ASSESSMENT MODELS; ANOPLOPOMA-FIMBRIA;
   JUVENILE SABLEFISH; MESOSCALE EDDIES; TAGGED SABLEFISH; PACIFIC SALMON;
   NORTHERN GULF; REGIME SHIFTS; VARIABILITY
AB In fisheries stock assessment, reliable estimation of year-class strength is often hindered by lack of data on early life history stages and limited knowledge of the underlying environmental processes influencing survival through these stages. One solution to improving these estimates of year-class strength or recruitment is to first develop regional indices representing the spatial and temporal extent of a hypothesized feature influencing a species' recruitment. These covariates should then be integrated within a population model where a variety of model selection techniques may be conducted to test for a reduction in recruitment uncertainty. The best selected model(s) may provide insight for developing hypotheses of mechanisms influencing recruitment. Here we consider the influence of a large-scale oceanographic feature, the North Pacific Polar Front, on recruitment of Alaska sablefish (Anoplopoma fimbria). Our working hypothesis is that advection of oceanic properties along the Polar Front and associated currents plays a key role in shaping the oceanographic climate of Alaskan waters and, hence, the environment that sablefish encounter during their early life history. As a first step in this investigation, we developed time series of sea surface temperature along the Polar Front mean path. We then integrated this data into the recruitment equations of the sablefish assessment base model. Model selection was based on a multistage hypothesis testing procedure combined with cross-validation and a retrospective analysis of prediction error. The impact of the best model was expressed in terms of increased precision of recruitment estimates and proportional changes in female spawning biomass for both current estimates and in future projections. The best model suggested that colder than average wintertime sea surface temperatures in the central North Pacific represent oceanic conditions that create positive recruitment events for sablefish. The incorporation of this index in the sablefish model provided moderate reduction in unexplained recruitment variability and increased future projections of spawning biomass in the medium term. Based on this result, we developed a conceptual model of three mechanisms that in combination form an ocean domain dynamic synergy (ODDS) which influences sablefish survival through the pelagic early life history stage. Successfully incorporating environmental time series into the sablefish assessment could establish a foundation for future ecosystem-based management and allow for more informed and efficient resource allocation to stakeholders. Published by Elsevier Ltd.
C1 [Shotwell, S. Kalei; Hanselman, Dana H.] Natl Ocean & Atmospher Adm, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs,Ted Stevens Marine Res Inst, Juneau, AK 99801 USA.
   [Belkin, Igor M.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA.
RP Shotwell, SK (reprint author), Natl Ocean & Atmospher Adm, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs,Ted Stevens Marine Res Inst, 17109 Pt Lena Loop Rd, Juneau, AK 99801 USA.
EM kalei.shotwell@noaa.gov
FU NOAA Fisheries and the Environment (FATE)
FX We would like to thank Dr. Lisa Eisner, Dr. Franz Mueter, and the
   scientists from other institutions who assisted with thoughtful comments
   and ideas in the paper review. Also we thank Phil Rigby, Dr. Jon
   Heifetz, Adam Moles, Jim Murphy, and Mark Zimmermann who provided many
   useful editorial comments to improve the project concepts and manuscript
   organization. Finally, we extend our gratitude to our primary funding
   source, NOAA Fisheries and the Environment (FATE). The findings and
   conclusions in the paper are those of the authors and do not necessarily
   represent the views of the National Marine Fisheries Service. Reference
   to trade names does not imply endorsement by the National Marine
   Fisheries Service, NOAA.
NR 67
TC 7
Z9 7
U1 0
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
EI 1879-0100
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD SEP
PY 2014
VL 107
BP 40
EP 53
DI 10.1016/j.dsr2.2012.08.024
PG 14
WC Oceanography
SC Oceanography
GA AR8SL
UT WOS:000343844600006
ER

PT J
AU Rosenzweig, C
   Solecki, W
AF Rosenzweig, Cynthia
   Solecki, William
TI Hurricane Sandy and adaptation pathways in New York: Lessons from a
   first-responder city
SO GLOBAL ENVIRONMENTAL CHANGE-HUMAN AND POLICY DIMENSIONS
LA English
DT Article
DE Adaptation pathways; Cities; Climate change; Resilience; Transformation
ID CLIMATE-CHANGE; INSURANCE; GAP
AB Two central issues of climate change have become increasingly evident: Climate change will significantly affect cities; and rapid global urbanization will increase dramatically the number of individuals, amount of critical infrastructure, and means of economic production that are exposed and vulnerable to dynamic climate risks. Simultaneously, cities in many settings have begun to emerge as early adopters of climate change action strategies including greenhouse gas mitigation and adaptation. The objective of this paper is to examine and analyze how officials of one city - the City of New York - have integrated a flexible adaptation pathways approach into the municipality's climate action strategy. This approach has been connected with the City's ongoing response to Hurricane Sandy, which struck in the October 2012 and resulted in damages worth more than US$19 billion. A case study narrative methodology utilizing the Wise et al. conceptual framework (see this volume) is used to evaluate the effectiveness of the flexible adaptation pathways approach in New York City. The paper finds that Hurricane Sandy serves as a "tipping point" leading to transformative adaptation due to the explicit inclusion of increasing climate change risks in the rebuilding effort. The potential for transferability of the approach to cities varying in size and development stage is discussed, with elements useful across cities including the overall concept of flexible adaptation pathways, the inclusion of the full metropolitan region in the planning process, and the co-generation of climate-risk information by stakeholders and scientists. Published by Elsevier Ltd.
C1 [Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
   [Solecki, William] CUNY Hunter Coll, CUNY Inst Sustainable Cities, New York, NY 10021 USA.
   [Solecki, William] CUNY Hunter Coll, Dept Geog, New York, NY 10021 USA.
   [Rosenzweig, Cynthia] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
RP Rosenzweig, C (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM crr2@columbia.edu; wsolecki@hunter.cuny.edu
NR 44
TC 23
Z9 23
U1 9
U2 50
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0959-3780
EI 1872-9495
J9 GLOBAL ENVIRON CHANG
JI Glob. Environ. Change-Human Policy Dimens.
PD SEP
PY 2014
VL 28
BP 395
EP 408
DI 10.1016/j.gloenvcha.2014.05.003
PG 14
WC Environmental Sciences; Environmental Studies; Geography
SC Environmental Sciences & Ecology; Geography
GA AR8QG
UT WOS:000343839100034
ER

PT J
AU Larour, E
   Khazendar, A
   Borstad, CP
   Seroussi, H
   Morlighem, M
   Rignot, E
AF Larour, E.
   Khazendar, A.
   Borstad, C. P.
   Seroussi, H.
   Morlighem, M.
   Rignot, E.
TI Representation of sharp rifts and faults mechanics in modeling ice shelf
   flow dynamics: Application to Brunt/Stancomb-Wills Ice Shelf, Antarctica
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
DE rift; fault; ice shelf; Brunt; Stancomb-Wills; flow; rheology
ID HARDENING MATERIAL; BOTTOM CREVASSES; EAST ANTARCTICA; COATS LAND;
   BREAK-UP; PROPAGATION; DEFORMATION; PENINSULA; COLLAPSE; FRACTURE
AB Ice shelves play a major role in buttressing ice sheet flow into the ocean, hence the importance of accurate numerical modeling of their stress regime. Commonly used ice flow models assume a continuous medium and are therefore complicated by the presence of rupture features (crevasses, rifts, and faults) that significantly affect the overall flow patterns. Here we apply contact mechanics and penalty methods to develop a new ice shelf flow model that captures the impact of rifts and faults on the rheology and stress distribution of ice shelves. The model achieves a best fit solution to satellite observations of ice shelf velocities to infer the following: (1) a spatial distribution of contact and friction points along detected faults and rifts, (2) a more realistic spatial pattern of ice shelf rheology, and (3) a better representation of the stress balance in the immediate vicinity of faults and rifts. Thus, applying the model to the Brunt/Stancomb-Wills Ice Shelf, Antarctica, we quantify the state of friction inside faults and the opening rates of rifts and obtain an ice shelf rheology that remains relatively constant everywhere else on the ice shelf. We further demonstrate that better stress representation has widespread application in examining aspects affecting ice shelf structure and dynamics including the extent of ice melange in rifts and the change in fracture configurations. All are major applications for better insight into the important question of ice shelf stability.
C1 [Larour, E.; Khazendar, A.; Seroussi, H.; Rignot, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
   [Borstad, C. P.] CALTECH, Pasadena, CA 91125 USA.
   [Morlighem, M.; Rignot, E.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA.
RP Larour, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM Eric.Larour@jpl.nasa.gov
RI Morlighem, Mathieu/O-9942-2014; Rignot, Eric/A-4560-2014; 
OI Morlighem, Mathieu/0000-0001-5219-1310; Rignot,
   Eric/0000-0002-3366-0481; Borstad, Christopher/0000-0001-6992-1770
FU NASA's Cryosphere Sciences Program; Modeling, Analysis and Prediction
   Program (MAP); President's and Director's Fund Program; NASA; National
   Aeronautics and Space Administration
FX This work was supported by grants from NASA's Cryosphere Sciences
   Program (E.L., A.K., M.M., and E.R.) as well as funding from the
   Modeling, Analysis and Prediction Program (MAP, E.L., and H.S.) and
   funding from the President's and Director's Fund Program (E.L.). C.B.
   was supported by an appointment to the NASA Postdoctoral Program at the
   Jet Propulsion Laboratory, administered by Oak Ridge Associated
   Universities through a contract with NASA followed by an appointment to
   the Jet Propulsion Laboratory / California Institute of Technology
   Postdoctoral Program. This work was performed at the Jet Propulsion
   Laboratory, California Institute of Technology, under a contract with
   the National Aeronautics and Space Administration, and at the University
   of California, Irvine, Department of Earth System Science. The
   RADARSAT-1, ERS 1/2 data sets used in this study, along with the
   GLAS/ICESat altimeter DEM of Antarctica can be found at the NASA
   Distributed Active Archive Center at the National Snow and Ice Data
   Center, Boulder, Colorado, USA. We want to also thank Michiel van den
   Broeke for the surface mass balance model of Antarctica used in this
   study.
NR 68
TC 3
Z9 3
U1 0
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9003
EI 2169-9011
J9 J GEOPHYS RES-EARTH
JI J. Geophys. Res.-Earth Surf.
PD SEP
PY 2014
VL 119
IS 9
BP 1918
EP 1935
DI 10.1002/2014JF003157
PG 18
WC Geosciences, Multidisciplinary
SC Geology
GA AR9EY
UT WOS:000343876500008
ER

PT J
AU Gregg, WW
   Rousseaux, CS
AF Gregg, Watson W.
   Rousseaux, Cecile S.
TI Decadal trends in global pelagic ocean chlorophyll: A new assessment
   integrating multiple satellites, in situ data, and models
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE trends; remote sensing; chlorophyll; models
ID LONG-TERM TRENDS; CLIMATE; PHYTOPLANKTON; PRODUCTIVITY; VARIABILITY
AB Quantifying change in ocean biology using satellites is a major scientific objective. We document trends globally for the period 1998-2012 by integrating three diverse methodologies: ocean color data from multiple satellites, bias correction methods based on in situ data, and data assimilation to provide a consistent and complete global representation free of sampling biases. The results indicated no significant trend in global pelagic ocean chlorophyll over the 15 year data record. These results were consistent with previous findings that were based on the first 6 years and first 10 years of the SeaWiFS mission. However, all of the Northern Hemisphere basins (north of 10 degrees latitude), as well as the Equatorial Indian basin, exhibited significant declines in chlorophyll. Trend maps showed the local trends and their change in percent per year. These trend maps were compared with several other previous efforts using only a single sensor (SeaWiFS) and more limited time series, showing remarkable consistency. These results suggested the present effort provides a path forward to quantifying global ocean trends using multiple satellite missions, which is essential if we are to understand the state, variability, and possible changes in the global oceans over longer time scales.
C1 [Gregg, Watson W.; Rousseaux, Cecile S.] NASA, Global Modeling & Assimilat Off, Greenbelt, MD 20770 USA.
   [Rousseaux, Cecile S.] Univ Space Res Assoc, Greenbelt, MD USA.
RP Gregg, WW (reprint author), NASA, Global Modeling & Assimilat Off, Greenbelt, MD 20770 USA.
EM watson.gregg@nasa.gov
RI Rousseaux, Cecile/E-8811-2012
OI Rousseaux, Cecile/0000-0002-3022-2988
FU NASA EOS program
FX We are grateful for the data from the SeaWiFS and MODIS-Aqua missions,
   the processing by the NASA Ocean Color team, in situ data collection by
   NODC, Atlantic Meridional Transect, NASA, individual investigators, and
   the NASA Center for Climate Simulation for computing time for the model
   and data assimilation. We thank Stephanie Henson, Vincent Vantrepotte,
   and David Siegel for permission to use their figures in Figure 7. This
   work was supported by the NASA EOS program. Data used in this analysis
   can be obtained at the NASA GES-DISC Giovanni web location
   http://gdata1.sci.gsfc.nasa.gov/daac-bin/G3/gui.cgi?instance_id=ocean_mo
   del (or search NOBM Giovanni).
NR 24
TC 22
Z9 22
U1 2
U2 23
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD SEP
PY 2014
VL 119
IS 9
BP 5921
EP 5933
DI 10.1002/2014JC010158
PG 13
WC Oceanography
SC Oceanography
GA AR9FW
UT WOS:000343879200019
ER

PT J
AU Moon, JH
   Song, YT
AF Moon, Jae-Hong
   Song, Y. Tony
TI Seasonal salinity stratifications in the near-surface layer from
   Aquarius, Argo, and an ocean model: Focusing on the tropical
   Atlantic/Indian Oceans
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE sea surface salinity; Aquarius; Argo; seasonal cycle; ocean circulation
   model; salinity stratification
ID INDIAN-OCEAN; MIXED-LAYER; SEA; VARIABILITY; AMAZON; SMOS; TEMPERATURE;
   CIRCULATION; SYSTEM; SPACE
AB A newly available sea surface salinity (SSS) measurement from Aquarius/SAC-D satellite reveals strong seasonal variability in the tropical Atlantic and Indian Oceans. The seasonal SSS variability at skin layer differs/agrees regionally in their amplitude from/with Argo-measured salinity at 5 m depth and model salinity at the top layer, indicating various characteristics of near-surface salinity stratifications. By comparing the three different salinity products, we have examined the near-surface salinity stratifications with emphasis on the dynamical processes that differ from one region to another. Our analysis shows that for the western part of tropical Atlantic and southern tropical Indian, a large amount of river runoff and/or surface freshwater significantly stratifies the surface layer above 5 m depth, resulting in the differences among the Aquarius, Argo, and model. Differently for the southern Arabian Sea, the surface water can be mixed down to the depth of 5 m due to seasonally reversing currents driven by monsoons, resulting in an agreement among the data sets. The comparison suggests that dynamical differences can lead to different vertical salinity stratifications locally, which explain the differences between the Aquarius observations in the first cm of the sea surface, the Argo measurements at the 5 m depth, and model's representation of the surface-layer averaged salinity.
C1 [Moon, Jae-Hong; Song, Y. Tony] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Moon, JH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Jae-Hong.Moon@jpl.nasa.gov
NR 38
TC 6
Z9 6
U1 2
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD SEP
PY 2014
VL 119
IS 9
BP 6066
EP 6077
DI 10.1002/2014JC009969
PG 12
WC Oceanography
SC Oceanography
GA AR9FW
UT WOS:000343879200027
ER

PT J
AU Tang, WQ
   Yueh, SH
   Fore, AG
   Hayashi, A
AF Tang, Wenqing
   Yueh, Simon H.
   Fore, Alexander G.
   Hayashi, Akiko
TI Validation of Aquarius sea surface salinity with in situ measurements
   from Argo floats and moored buoys
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE Aquarius; sea surface salinity; validation; Argo; moored buoy
ID OCEAN ALGORITHM; D MISSION; ARRAY; TEMPERATURE; PREDICTION; CHALLENGE;
   PROGRESS; PIRATA
AB We validate sea surface salinity (SSS) retrieved from Aquarius instrument on SAC-D satellite with in situ measurements by Argo floats and moored buoy arrays. We assess the error structure of three Aquarius SSS products: the standard product processed by Aquarius Data Processing System (ADPS) and two data sets produced at the Jet Propulsion Laboratory (JPL): the Combined Active-Passive algorithm with and without rain correction, CAP and CAP_RC, respectively. We examine the effect of various filters to prevent unreliable point retrievals from entering Level 3 averaging, such as land or ice contamination, radio frequency interference (RFI), and cold water. Our analyses show that Aquarius SSS agrees well with Argo in a monthly average sense between 40 degrees S and 40 degrees N except in the Eastern Pacific Fresh Pool and Amazon River outflow. Buoy data within these regions show excellent agreement with Aquarius but have discrepancies with the Argo gridded products. Possible reasons include strong near-surface stratification and sampling problems in Argo in regions with significant western boundary currents. We observe large root-mean-square (RMS) difference and systematic negative bias between ADPS and Argo in the tropical Indian Ocean and along the Southern Pacific Convergence Zone. Excluding these regions removes the suspicious seasonal peak in the monthly RMS difference between the Aquarius SSS products and Argo. Between 40 degrees S and 40 degrees N, the RMS difference for CAP is less than 0.22 PSU for all 28 months, CAP_RC has essentially met the monthly 0.2 PSU accuracy requirement, while that for ADPS fluctuates between 0.22 and 0.3 PSU.
C1 [Tang, Wenqing; Yueh, Simon H.; Fore, Alexander G.; Hayashi, Akiko] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Tang, WQ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Wenqing.Tang@jpl.nasa.gov
NR 28
TC 23
Z9 25
U1 2
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD SEP
PY 2014
VL 119
IS 9
BP 6171
EP 6189
DI 10.1002/2014JC010101
PG 19
WC Oceanography
SC Oceanography
GA AR9FW
UT WOS:000343879200033
ER

PT J
AU Mohan, S
   Miller, DW
AF Mohan, Swati
   Miller, David W.
TI Dynamic Control Model Calculation: A Model Generation Architecture for
   Autonomous On-Orbit Assembly
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB Autonomous on-orbit assembly is a key technology that can enable many space applications in a more cost-effective and lower risk manner than human-assisted assembly. During an assembly sequence, an assembler robot can undergo multiple configurations as it attaches to and releases individual modules. This paper addresses how to account for the mass and stiffness property variations that occur with changes in configuration. Proper model generation for each configuration is critical to maintain control system stability and efficiency. A design, called dynamic control model calculation, is presented in this paper to address a gap where models are aggregated online based on module mass property information. This design uses module information obtained at the time of attachment to generate the model for the current configuration onboard. The design, both framework and algorithm parameterization, has been successfully implemented and validated on hardware. Hardware results show a tracking error performance improvement when the correct model of the system is used in the control system over an incorrect model. Dynamic control model calculation successfully balances a priori knowledge about the possible configurations with identification of the model onboard.
C1 [Mohan, Swati] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Miller, David W.] MIT, Cambridge, MA 02139 USA.
RP Mohan, S (reprint author), 4800 Oak Grove Dr,Mail Stop 198-326, Pasadena, CA USA.
FU NASA Small Business Innovation Research [NNM07AA22C]; NASA Harriet G.
   Jenkins Predoctoral Fellowship Program
FX This work was performance primarily under NASA Small Business Innovation
   Research Contract NNM07AA22C Self-Assembling Wireless Autonomous
   Reconfigurable Modules, and the NASA Harriet G. Jenkins Predoctoral
   Fellowship Program. The authors gratefully thank the sponsors for their
   generous support that enabled this research. This research was performed
   at the Massachusetts Institute of Technology Space Systems Laboratory
   and was supervised by David W. Miller. The authors also thank the
   Synchronized Position Hold, Engage, Reorient, Experimental Satellites
   team for their collaboration and support. Thank you to Scott Ploen and
   Oscar Alvarez-Salazar for reviewing the paper and providing constructive
   feedback.
NR 25
TC 2
Z9 2
U1 1
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-OCT
PY 2014
VL 51
IS 5
BP 1430
EP 1453
DI 10.2514/1.A32581
PG 24
WC Engineering, Aerospace
SC Engineering
GA AR8AH
UT WOS:000343797500005
ER

PT J
AU Restrepo, CI
   Hurtado, JE
AF Restrepo, Carolina I.
   Hurtado, John E.
TI Tool for Rapid Analysis of Monte Carlo Simulations
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID MUTUAL INFORMATION; DESCENT; ENTRY
AB During the early design phases of any complex aerospace system, Monte Carlo simulations are performed and analyzed to better understand the physics of the problem and to identify design variables that must be either changed or studied further. The Tool for Rapid Analysis of Monte Carlo simulations was developed to assist engineers in the postprocessing of Monte Carlo simulation results. This work combines two pattern-recognition algorithms, kernel density estimation and K nearest neighbors, into a practical analysis tool that ranks influential variables given a specific failure metrics. The Tool for Rapid Analysis of Monte Carlo simulations uses a failure metric to separate the simulation results into two groups: successful and failed simulation runs. The kernel density estimation and K nearest neighbors algorithms are used to estimate probability density functions of the two different groups of data, which are then used to calculate a cost function that quantifies the relative influence of each design variable. In addition to producing a ranking of influential design variables, the Tool for Rapid Analysis of Monte Carlo simulations can rank combinations of up to four design variables in the form of differences and ratios. This paper shows results for a dynamical system with an analytical solution to demonstrate how these methods can identify failure regions in a Monte Carlo data set.
C1 [Restrepo, Carolina I.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
   [Hurtado, John E.] Texas A&M Univ, Dept Aerosp Engn, College Stn, TX 77843 USA.
RP Restrepo, CI (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
FU Integrated Guidance, Navigation, and Control Analysis Branch at NASA
   Johnson Space Center
FX The authors wish to acknowledge the support of the Integrated Guidance,
   Navigation, and Control Analysis Branch at NASA Johnson Space Center.
   Any opinions, findings and conclusions, or recommendations in this
   material are those of the authors and do not necessarily reflect the
   views of NASA.
NR 32
TC 0
Z9 0
U1 3
U2 4
PU AMER INST AERONAUTICS  ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2014
VL 51
IS 5
BP 1564
EP 1575
DI 10.2514/1.A32679
PG 12
WC Engineering, Aerospace
SC Engineering
GA AR8AH
UT WOS:000343797500015
ER

PT J
AU Stuart, JR
   Howell, KC
   Wilson, RS
AF Stuart, Jeffrey R.
   Howell, Kathleen C.
   Wilson, Roby S.
TI Automated Design of Propellant-Optimal, Low-Thrust Trajectories for
   Trojan Asteroid Tours
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID OPTIMIZATION; ORBITS
AB The sun-Jupiter Trojan asteroid swarms are targets of interest for robotic spacecraft missions, where low-thrust propulsion systems offer a viable approach for realizing tours of these asteroids. This investigation introduces a novel scheme for the automated creation of prospective tours under the natural dynamics of a multibody regime with thrust supplied by a variable-specific-impulse engine. The procedure approximates tours by combining independently generated fuel-optimal rendezvous arcs between asteroid pairs into a series of trajectory legs. Propellant costs as well as departure and arrival times are estimated from the performance of the individual thrust arcs. Tours of interest are readily constructed in higher-fidelity models, and options for the end-to-end trajectories are easily assessed. In this investigation, scenarios where constant and varying-power sources are available to the low-thrust engine are explored. In general, the automation procedure rapidly generates a large number of potential tours and supplies reasonable cost estimates for preliminary baseline mission design. Computational aspects of the design procedure are automated such that end-to-end trajectories are generated with a minimum of human interaction after key elements associated with a proposed mission concept are specified.
C1 [Stuart, Jeffrey R.; Howell, Kathleen C.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
   [Wilson, Roby S.] CALTECH, Jet Prop Lab, Inner Planets Mission Anal Grp, Miss Design & Nav Sect, Pasadena, CA 91109 USA.
RP Stuart, JR (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, 701 West Stadium Ave, W Lafayette, IN 47907 USA.
FU Purdue Research Foundation; NASA Office of the Chief Technologist's
   Space Technology Research Fellowship, NASA [NNX12AM61H]
FX The authors appreciate the thoughtful comments and suggestions from the
   editor and anonymous reviewers that have significantly improved the
   manuscript. This work was conducted at Purdue University and the Jet
   Propulsion Laboratory and is supported by the Purdue Research Foundation
   and a NASA Office of the Chief Technologist's Space Technology Research
   Fellowship, NASA grant NNX12AM61H. Many thanks to Wayne Schlei, who
   helped immensely with the trajectory images, and the technical personnel
   of the Jet Propulsion Laboratory, Mission Design and Navigation Section.
NR 22
TC 3
Z9 3
U1 1
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-OCT
PY 2014
VL 51
IS 5
BP 1631
EP 1647
DI 10.2514/1.A32748
PG 17
WC Engineering, Aerospace
SC Engineering
GA AR8AH
UT WOS:000343797500020
ER

PT J
AU Spak, KS
   Agnes, GS
   Inman, DJ
AF Spak, Kaitlin S.
   Agnes, Gregory S.
   Inman, Daniel J.
TI Bakeout Effects on Dynamic Response of Spaceflight Cables
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID EXPERIMENTAL VALIDATION; SPACE STRUCTURES
AB Spaceflight cables are investigated to determine the effect of bakeout on their dynamic response, including resonant frequencies and damping ratios. The addition of cable harnesses to spacecraft structures can affect the dynamic response of the entire structure, especially for lightweight structures with high cable mass ratios. Bakeout, a heat and vacuum treatment that spaceflight components must undergo, may change the dynamic stiffness of flight cables and thus the dynamics of the cabled host structure. Bakeout effects are examined by experimentally identifying natural frequencies and damping values for spaceflight cables before and after the bakeout process. After bakeout, the first natural frequency decreases by an average of 14% for all single-strand cables and by 24% for multistrand cables. The second natural frequency decreases by 8 to 17% for all cables. Bakeout also increases the damping percentage for single and multistrand cables. These results show that bakeout affects the dynamic response of spaceflight cables significantly and should be taken into account when using cable data for design purposes.
C1 [Spak, Kaitlin S.] Virginia Polytech Inst & State Univ, Dept Mech Engn, Blacksburg, VA 24060 USA.
   [Agnes, Gregory S.] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA.
   [Inman, Daniel J.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA.
RP Spak, KS (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA.
FU NASA Space Technology Research Fellowship program; Virginia Space Grant
   Consortium; Southern California Braiding, Inc.; U.S. Air Force Office of
   Scientific Research [FA9550-10-1-0427]; NASA
FX K. Spak thanks the NASA Space Technology Research Fellowship program for
   generous support and the Virginia Space Grant Consortium for additional
   funding as well as Southern California Braiding, Inc., for providing
   flight cables at cost. D. Inman gratefully acknowledges the support of
   U.S. Air Force Office of Scientific Research grant number
   FA9550-10-1-0427 monitored by David Stargel. Part of this research was
   carried out at the Jet Propulsion Laboratory, California Institute of
   Technology, under a contract with NASA.
NR 18
TC 2
Z9 2
U1 1
U2 2
PU AMER INST AERONAUTICS  ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD SEP-OCT
PY 2014
VL 51
IS 5
BP 1721
EP 1734
DI 10.2514/1.A32780
PG 14
WC Engineering, Aerospace
SC Engineering
GA AR8AH
UT WOS:000343797500027
ER

PT J
AU Rastatter, L
   Toth, G
   Kuznetsova, MM
   Pulkkinen, AA
AF Rastaetter, Lutz
   Toth, Gabor
   Kuznetsova, Maria M.
   Pulkkinen, Antti A.
TI CalcDeltaB: An efficient postprocessing tool to calculate ground-level
   magnetic perturbations from global magnetosphere simulations
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE numerical simulation; magnetic perturbations; real-time processing
ID IONOSPHERE; FIELD; MODEL
AB Ground magnetic field variations can induce electric currents on long conductor systems such as high-voltage power transmission systems. The extra electric currents can interfere with normal operation of these conductor systems; and thus, there is a great need for better specification and prediction of the field perturbations. In this publication we present CalcDeltaB, an efficient postprocessing tool to calculate magnetic perturbations B at any position on the ground from snapshots of the current systems that are being produced by first-principle models of the global magnetosphere-ionosphere system. This tool was developed during the recent dB/dt modeling challenge at the Community Coordinated Modeling Center that compared magnetic perturbations and their derivative with observational results. The calculation tool is separate from each of the magnetosphere models and ensures that the B computation method is uniformly applied, and that validation studies using B compare the performance of the models rather than the combination of each model and a built-in B computation tool that may exist. Using the tool, magnetic perturbations on the ground are calculated from currents in the magnetosphere, from field-aligned currents between magnetosphere and ionosphere, and the Hall and Pedersen currents in the ionosphere. The results of the new postprocessing tool are compared with B calculations within the Space Weather Modeling Framework model and are in excellent agreement. We find that a radial resolution of 1/30R(E) is fine enough to represent the contribution to B from the region of field-aligned currents.
C1 [Rastaetter, Lutz; Kuznetsova, Maria M.; Pulkkinen, Antti A.] NASA, Community Coordinated Modeling Ctr, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Toth, Gabor] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA.
RP Rastatter, L (reprint author), NASA, Community Coordinated Modeling Ctr, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Lutz.Rastaetter@nasa.gov
RI Toth, Gabor/B-7977-2013; Rastaetter, Lutz/D-4715-2012
OI Toth, Gabor/0000-0002-5654-9823; Rastaetter, Lutz/0000-0002-7343-4147
NR 18
TC 5
Z9 5
U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD SEP
PY 2014
VL 12
IS 9
BP 553
EP 565
DI 10.1002/2014SW001083
PG 13
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
   Atmospheric Sciences
GA AR8AK
UT WOS:000343797800001
ER

PT J
AU Buson, S
   Longo, F
   Larsson, S
   Cutini, S
   Finke, J
   Ciprini, S
   Ojha, R
   D'Ammando, F
   Donato, D
   Thompson, DJ
   Desiante, R
   Bastieri, D
   Wagner, S
   Hauser, M
   Fuhrmann, L
   Dutka, M
   Muller, C
   Kadler, M
   Angelakis, E
   Zensus, JA
   Stevens, J
   Blanchard, JM
   Edwards, PG
   Lovell, JEJ
   Gurwell, MA
   Wehrle, AE
   Zook, A
AF Buson, S.
   Longo, F.
   Larsson, S.
   Cutini, S.
   Finke, J.
   Ciprini, S.
   Ojha, R.
   D'Ammando, F.
   Donato, D.
   Thompson, D. J.
   Desiante, R.
   Bastieri, D.
   Wagner, S.
   Hauser, M.
   Fuhrmann, L.
   Dutka, M.
   Mueller, C.
   Kadler, M.
   Angelakis, E.
   Zensus, J. A.
   Stevens, J.
   Blanchard, J. M.
   Edwards, P. G.
   Lovell, J. E. J.
   Gurwell, M. A.
   Wehrle, A. E.
   Zook, A.
TI Unusual flaring activity in the blazar PKS 1424-418 during 2008-2011
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; radiation mechanisms: non-thermal; quasars:
   individual: PKS 1424-418; gamma rays: galaxies; galaxies: jets
ID LARGE-AREA TELESCOPE; GAMMA-RAY FLARE; GALACTIC NUCLEI; COMPTON
   ANALYSIS; SOURCE CATALOG; RADIO-SOURCES; 3C 454.3; VARIABILITY;
   EMISSION; MISSION
AB Context. Blazars are a subset of active galactic nuclei (AGN) with jets that are oriented along our line of sight. Variability and spectral energy distribution (SED) studies are crucial tools for understanding the physical processes responsible for observed AGN emission.
   Aims. We report peculiar behavior in the bright gamma-ray blazar PKS 1424 418 and use its strong variability to reveal information about the particle acceleration and interactions in the jet.
   Methods. Correlation analysis of the extensive optical coverage by the ATOM telescope and nearly continuous gamma-ray coverage by the Fermi Large Area Telescope is combined with broadband, time-dependent modeling of the SED incorporating supplemental information from radio and X-ray observations of this blazar.
   Results. We analyse in detail four bright phases at optical-GeV energies. These flares of PKS 1424-418 show high correlation between these energy ranges, with the exception of one large optical flare that coincides with relatively low gamma-ray activity. Although the optical/gamma-ray behavior of PKS 1424-418 shows variety, the multiwavelength modeling indicates that these differences can largely be explained by changes in the flux and energy spectrum of the electrons in the jet that are radiating. We find that for all flares the SED is adequately represented by a leptonic model that includes inverse Compton emission from external radiation fields with similar parameters.
   Conclusions. Detailed studies of individual blazars like PKS 1424 418 during periods of enhanced activity in different wavebands are helping us identify underlying patterns in the physical parameters in this class of AGN.
C1 [Buson, S.; Bastieri, D.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
   [Buson, S.; Bastieri, D.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
   [Longo, F.; Desiante, R.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
   [Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
   [Larsson, S.] Stockholm Univ, Dept Phys, Alballova, S-10691 Stockholm, Sweden.
   [Larsson, S.] Alballova, Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden.
   [Larsson, S.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden.
   [Cutini, S.; Ciprini, S.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy.
   [Cutini, S.; Ciprini, S.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Rome, Italy.
   [Finke, J.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
   [Ojha, R.; Donato, D.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [D'Ammando, F.; Kadler, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
   [Donato, D.] Ctr Res & Explorat Space Sci & Technol CRESST, Greenbelt, MD 20771 USA.
   [Donato, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
   [Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
   [Wagner, S.; Hauser, M.] Heidelberg Univ, D-69117 Heidelberg, Germany.
   [Fuhrmann, L.; Angelakis, E.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
   [Dutka, M.] Catholic Univ Amer, Washington, DC 20064 USA.
   [Mueller, C.; Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
   [Mueller, C.; Kadler, M.] Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany.
   [Kadler, M.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
   [Kadler, M.] Univ Space Res Assoc USRA, Columbia, MD 21044 USA.
   [Stevens, J.] CSIRO Astron & Space Sci, ATNF, Narrabri, NSW 2390, Australia.
   [Blanchard, J. M.; Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
   [Edwards, P. G.] CSIRO Astron & Space Sci, ATNF, Epping, NSW 1710, Australia.
   [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Wehrle, A. E.] Space Sci Inst, Boulder, CO USA.
   [Zook, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Buson, S (reprint author), Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
EM sara.buson@pd.infn.it; francesco.longo@trieste.infn.it
OI Bastieri, Denis/0000-0002-6954-8862; Angelakis,
   Emmanouil/0000-0001-7327-5441; Kadler, Matthias/0000-0001-5606-6154
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 in Italy; K. A.
   Wallenberg Foundation in Sweden; German Deutsche Forschungsgemeinschaft,
   DFG [Ts 17/2-1]; Commonwealth of Australia; Smithsonian Institution;
   Academia Sinica; NASA through Fermi Guest Investigator grants
   [NNH10ZDA001N, NNH09ZDA001N];  [6090777]
FX The Fermi LAT Collaboration acknowledges generous on-going support from
   a number of agencies and institutes that have supported both the
   development and the operation of the LAT as well as scientific data
   analysis. These include the National Aeronautics and Space
   Administration and the Department of Energy in the United States, the
   Commissariat a l'Energie Atomique and the Centre National de la
   Recherche Scientifique/Institut National de Physique Nucleaire et de
   Physique des Particules in France, the Agenzia Spaziale Italiana and the
   Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
   Education, Culture, Sports, Science and Technology (MEXT), High Energy
   Accelerator Research Organization (KEK) and Japan Aerospace Exploration
   Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
   Research Council and the Swedish National Space Board in Sweden.
   Additional support for science analysis during the operations phase from
   the following agencies is also gratefully acknowledged: the Istituto
   Nazionale di Astrofisica in Italy and the K. A. Wallenberg Foundation in
   Sweden for providing a grant in support of a Royal Swedish Academy of
   Sciences Research fellowship for J.C. Part of this work was supported by
   the German Deutsche Forschungsgemeinschaft, DFG project number Ts
   17/2-1. The Australian Long Baseline Array and the Australia Telescope
   Compact Array are part of the Australia Telescope National Facility
   which is funded by the Commonwealth of Australia for operation as a
   National Facility managed by CSIRO. The Submillimeter Array is a joint
   project between the Smithsonian Astrophysical Observatory and the
   Academia Sinica Institute of Astronomy and Astrophysics and is funded by
   the Smithsonian Institution and the Academia Sinica. This research was
   funded in part by NASA through Fermi Guest Investigator grants
   NNH09ZDA001N and NNH10ZDA001N. 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. We thank Neil Gehrels and the Swift team for
   scheduling our Target of Opportunity requests. This research was enabled
   in part through Swift Guest Investigator grants 6090777. We thank Silvia
   Raino for useful comments and suggestions.
NR 61
TC 4
Z9 4
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
   FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2014
VL 569
AR A40
DI 10.1051/0004-6361/201423367
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8PZ
UT WOS:000343092100038
ER

PT J
AU Castro, M
   D'Amico, F
   Braga, J
   Maiolino, T
   Pottschmidt, K
   Wilms, J
AF Castro, M.
   D'Amico, F.
   Braga, J.
   Maiolino, T.
   Pottschmidt, K.
   Wilms, J.
TI Confirming the thermal Comptonization model for black hole X-ray
   emission in the low-hard state
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE radiation mechanisms: non-thermal; radiation mechanisms: thermal;
   X-rays: stars
ID PHOTON IMAGING CAMERA; 1E 1740.7-2942; GALACTIC-CENTER; XMM-NEWTON;
   1E-1740.7-2942; 1E1740.7-2942; BINARIES; SPECTRUM; REFLECTION; IMAGER
AB Hard X-ray spectra of black hole binaries in the low/hard state are well modeled by thermal Comptonization of soft seed photons by a corona-type region with kT similar to 50 keV and optical depth around 1. Previous spectral studies of 1E 1740.7-2942, including both the soft and the hard X-ray bands, were always limited by gaps in the spectra or by a combination of observations with imaging and non-imaging instruments. In this study, we have used three rare nearly-simultaneous observations of 1E 1740.7-1942 by both XMM-Newton and INTEGRAL satellites to combine spectra from four different imaging instruments with no data gaps, and we successfully applied the Comptonization scenario to explain the broadband X-ray spectra of this source in the low/hard state. For two of the three observations, our analysis also shows that, models including Compton reflection can adequately fit the data, in agreement with previous reports. We show that the observations can also be modeled by a more detailed Comptonization scheme. Furthermore, we find the presence of an iron K-edge absorption feature in one occasion, which confirms what had been previously observed by Suzaku. Our broadband analysis of this limited sample shows a rich spectral variability in 1E 1740.7 2942 at the low/hard state, and we address the possible causes of these variations. More simultaneous soft/hard X-ray observations of this system and other black-hole binaries would be very helpful in constraining the Comptonization scenario and shedding more light on the physics of these systems.
C1 [Castro, M.; D'Amico, F.; Braga, J.] INPE, BR-12227010 Sao Jose Dos Campos, Brazil.
   [Maiolino, T.] Univ Ferrara, Phys Earth Sci Dept, I-44122 Ferrara, Italy.
   [Maiolino, T.] Univ Nice Sophia Antipolis, F-06108 Nice, France.
   [Pottschmidt, K.] NASA GSFC, Cresst, Greenbelt, MD USA.
   [Pottschmidt, K.] UMBC, Baltimore, MD USA.
   [Wilms, J.] Univ Erlangen Nurnberg, Remeis Observ, D-96049 Bamberg, Germany.
   [Wilms, J.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany.
RP Castro, M (reprint author), INPE, BR-12227010 Sao Jose Dos Campos, Brazil.
EM castro@das.inpe.br; damico@das.inpe.br; braga@das.inpe.br;
   maiolino@fe.infn.it; katja@milkyway.gsfc.nasa.gov;
   joern.wilms@sternwarte.uni-erlangen.de
RI Wilms, Joern/C-8116-2013; Castro Avila, Manuel Antonio/M-7492-2014
OI Wilms, Joern/0000-0003-2065-5410; 
FU CAPES/Brazil; COSPAR Program for Capacity Building Fellowship
FX M.C. gratefully acknowledges CAPES/Brazil for support. M. C. gratefully
   acknowledges Mariano Mendez at the Kapteyn Astronomical Institute
   (Groningen-The Netherlands) host in a visit in the period of September -
   October/2012, sponsored by the COSPAR Program for Capacity Building
   Fellowship, for helpful discussions in the subject of this study. M. C.
   and F. D. acknowledges Raimundo Lopes de Oliveira Filho for early
   guidance in XMM data analysis issues. F. D. acknowledges Tomaso Belloni
   for helpful discussions. We deeply acknowledge Andrzej Zdziarski, our
   referee, for superb comments and for helping us in improving the quality
   of this study.
NR 33
TC 3
Z9 3
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
   FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2014
VL 569
AR A82
DI 10.1051/0004-6361/201323290
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8PZ
UT WOS:000343092100030
ER

PT J
AU Catalano, A
   Ade, P
   Atik, Y
   Benoit, A
   Breele, E
   Bock, JJ
   Camus, P
   Chabot, M
   Charra, M
   Crill, BP
   Coron, N
   Coulais, A
   Desert, FX
   Fauvet, L
   Giraud-Heraud, Y
   Guillaudin, O
   Holmes, W
   Jones, WC
   Lamarre, JM
   Macias-Perez, J
   Martinez, M
   Miniussi, A
   Monfardini, A
   Pajot, F
   Patanchon, G
   Pelissier, A
   Piat, M
   Puget, JL
   Renault, C
   Rosset, C
   Santos, D
   Sauve, A
   Spencer, LD
   Sudiwala, R
AF Catalano, A.
   Ade, P.
   Atik, Y.
   Benoit, A.
   Breele, E.
   Bock, J. J.
   Camus, P.
   Chabot, M.
   Charra, M.
   Crill, B. P.
   Coron, N.
   Coulais, A.
   Desert, F-X
   Fauvet, L.
   Giraud-Heraud, Y.
   Guillaudin, O.
   Holmes, W.
   Jones, W. C.
   Lamarre, J. -M.
   Macias-Perez, J.
   Martinez, M.
   Miniussi, A.
   Monfardini, A.
   Pajot, F.
   Patanchon, G.
   Pelissier, A.
   Piat, M.
   Puget, J. -L.
   Renault, C.
   Rosset, C.
   Santos, D.
   Sauve, A.
   Spencer, L. D.
   Sudiwala, R.
TI Impact of particles on the Planck HFI detectors: Ground-based
   measurements and physical interpretation
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE instrumentation: detectors; space vehicles: instruments; methods: data
   analysis; cosmic background radiation; cosmic rays
ID HIGH-FREQUENCY INSTRUMENT; BOLOMETERS; PERFORMANCE; READOUT
AB The Planck High Frequency Instrument (HFI) surveyed the sky continuously from August 2009 to January 2012. Its noise and sensitivity performance were excellent (from 11 to 40 aW Hz(-1)), but the rate of cosmic-ray impacts on the HFI detectors was unexpectedly higher than in other instruments. Furthermore, collisions of cosmic rays with the focal plane produced transient signals in the data (glitches) with a wide range of characteristics and a rate of about one glitch per second. A study of cosmic-ray impacts on the HFI detector modules has been undertaken to categorize and characterize the glitches, to correct the HFI time-ordered data, and understand the residual effects on Planck maps and data products. This paper evaluates the physical origins of glitches observed by the HFI detectors. To better understand the glitches observed by HFI in flight, several ground-based experiments were conducted with flight-spare HFI bolometer modules. The experiments were conducted between 2010 and 2013 with HFI test bolometers in different configurations using varying particles and impact energies. The bolometer modules were exposed to 23 MeV protons from the Orsay IPN Tandem accelerator, and to Am-241 and Cm-244 alpha-particle and Fe-55 radioactive X-ray sources. The calibration data from the HFI ground-based preflight tests were used to further characterize the glitches and compare glitch rates with statistical expectations under laboratory conditions. Test results provide strong evidence that the dominant family of glitches observed in flight are due to cosmic-ray absorption by the silicon die substrate on which the HFI detectors reside. Glitch energy is propagated to the thermistor by ballistic phonons, while thermal diffusion also contributes. The average ratio between the energy absorbed, per glitch, in the silicon die and that absorbed in the bolometer is equal to 650. We discuss the implications of these results for future satellite missions, especially those in the far-infrared to submillimeter and millimeter regions of the electromagnetic spectrum.
C1 [Catalano, A.; Guillaudin, O.; Macias-Perez, J.; Pelissier, A.; Renault, C.; Santos, D.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, Inst Natl Polytech Grenoble, CNRS,IN2P3, F-38026 Grenoble, France.
   [Ade, P.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
   [Atik, Y.; Charra, M.; Coron, N.; Martinez, M.; Miniussi, A.; Pajot, F.; Puget, J. -L.] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR 8617, F-91405 Orsay, France.
   [Benoit, A.; Camus, P.; Monfardini, A.] Univ Grenoble 1, CNRS, Inst Neel, F-38042 Grenoble, France.
   [Breele, E.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.] Univ Paris 07, CNRS, UMR 7164, F-75205 Paris, France.
   [Bock, J. J.] CALTECH, Pasadena, CA 91125 USA.
   [Bock, J. J.; Crill, B. P.; Holmes, W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Chabot, M.] Univ Paris 11, IPN Inst Phys Nucl, CNRS, IN2P3, F-91406 Orsay, France.
   [Coulais, A.; Lamarre, J. -M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France.
   [Desert, F-X] Univ Grenoble 1, IPAG Inst Planetol & Astrophys Grenoble, CNRS, INSU,UMR 5274, F-38041 Grenoble, France.
   [Fauvet, L.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands.
   [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
   [Sauve, A.] CNRS, IRAP, F-31028 Toulouse 4, France.
RP Catalano, A (reprint author), Univ Grenoble 1, Lab Phys Subatom & Cosmol, Inst Natl Polytech Grenoble, CNRS,IN2P3, 53 Rue Martyrs, F-38026 Grenoble, France.
EM catalano@lpsc.in2p3.fr
RI Martinez, Maria/K-4827-2012
OI Martinez, Maria/0000-0002-9043-4691
FU ESA member states (in particular the lead countries France and Italy);
   NASA(USA)
FX Planck (http://www.esa.int/Planck) is a project of the European Space
   Agency (ESA) with instruments provided by two scientific consortia
   funded by ESA member states (in particular the lead countries France and
   Italy), with contributions from NASA(USA) and telescope reflectors
   provided by a collaboration between ESA and a scientific consortium led
   and funded by Denmark.
NR 41
TC 6
Z9 6
U1 1
U2 5
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
   FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2014
VL 569
AR A88
DI 10.1051/0004-6361/201423868
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8PZ
UT WOS:000343092100069
ER

PT J
AU Cox, NLJ
   Cami, J
   Kaper, L
   Ehrenfreund, P
   Foing, BH
   Ochsendorf, BB
   van Hooff, SHM
   Salama, F
AF Cox, N. L. J.
   Cami, J.
   Kaper, L.
   Ehrenfreund, P.
   Foing, B. H.
   Ochsendorf, B. B.
   van Hooff, S. H. M.
   Salama, F.
TI VLT/X-Shooter survey of near-infrared diffuse interstellar bands
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: lines and bands; dust, extinction; line: identification; line:
   profiles
ID POLYCYCLIC AROMATIC-HYDROCARBONS; MOLECULAR CLOUDS; SPECTROSCOPY;
   ABSORPTION; C-60(+); DIB; IDENTIFICATION; SPECTROGRAPH; CONSTRAINTS;
   FEATURES
AB Context. The unknown identity of the diffuse interstellar band (DIB) carriers poses one of the longest standing unresolved problems in astrophysics. While the presence, properties, and behaviour of hundreds of optical DIBs between 4000 angstrom and 9000 angstrom have been well established, information on DIBs in both the ultra-violet and near-infrared (NIR) ranges is limited.
   Aims. In this paper, we present a spectral survey of the NIR range, from 0.9 mu m to 2.5 mu m. Our observations were designed to detect new DIBs, confirm previously proposed NIR DIBs, and characterise their behaviour with respect to known line-of-sight properties (including the optical DIBs present in our spectra).
   Methods. Using the X-Shooter instrument mounted on the ESO Very Large Telescope (VLT) we obtained medium-resolution spectra of eight known DIB targets and one telluric reference star, from 3000 angstrom to 25 000 angstrom in one shot.
   Results. In addition to the known 9577, 9632, 10 780, 11 797, and 13 175 angstrom NIR DIBs, we confirm 9 out of the 13 NIR DIBs that were presented by Geballe et al. (2011, Nature, 479, 200). Furthermore, we report 11 new NIR DIB candidates. The strengths of the strongest NIR DIBs show a general correlation with reddening, h((B-V)), but with a large scatter. Several NIR DIBs are more strongly correlated with the 5780 angstrom DIB strength than with E(B-V); this is especially the case for the 15 268 angstrom DIB. The NIR DIBs are strong: the summed equivalent widths of the five strongest NIR DIBs represent a small percent of the total equivalent width of the entire average DIB spectrum (per unit reddening). The NIR DIBs towards the translucent cloud HD 147889 are all weak with respect to the general trend. No direct match was found between observed NIR DIBs and laboratory matrix-isolation spectroscopic data of polycyclic aromatic hydrocarbons (PAHs).
   Conclusions. The strong correlation between the 5780 15 268 DIB pair implies that (Nf)(5780)/(Nf)(15268) = 14. However, the reduced strength of the 15 268 angstrom DIB in HD 147889 rules out a common carrier for these two DIBs. Since the ionisation fraction for small PAHs in this translucent cloud is known to be low compared to diffuse clouds, the weakness of the 15 268 angstrom DIB suggests that an ionised species could be the carrier of this NIR DIB.
C1 [Cox, N. L. J.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
   [Cami, J.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
   [Cami, J.] SETI Inst, Mountain View, CA 94043 USA.
   [Kaper, L.; van Hooff, S. H. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands.
   [Ehrenfreund, P.] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA.
   [Foing, B. H.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands.
   [Ochsendorf, B. B.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
   [Salama, F.] NASA AMES Res Ctr, Mountain View, CA USA.
RP Cox, NLJ (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D,Bus 2401, B-3001 Louvain, Belgium.
EM nick.cox@ster.kuleuven.be
RI Salama, Farid/A-8787-2009
OI Salama, Farid/0000-0002-6064-4401
FU Natural Sciences and Engineering Council of Canada (NSERC)
FX We thank the referee for a thorough reading of the manuscript and
   several insightful comments that improved the paper. N.L.J.C. thanks the
   staff at Paranal for their help in optimising the execution of our
   programme, and X-Shooter instrument scientists at ESO for assistance in
   data handling issues. J.C. acknowledges support from the Natural
   Sciences and Engineering Council of Canada (NSERC). We thank Lucas
   Ellerbroek for guidance in using Spextool to correct the data for
   telluric absorption lines. This research has made use of the Simbad
   database operated by CDS in Strasbourg.
NR 40
TC 9
Z9 9
U1 4
U2 8
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
   FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2014
VL 569
AR A117
DI 10.1051/0004-6361/201323061
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8PZ
UT WOS:000343092100026
ER

PT J
AU Merin, B
   Ardila, DR
   Ribas, A
   Bouy, H
   Bryden, G
   Stapelfeldt, K
   Padgett, D
AF Merin, Bruno
   Ardila, David R.
   Ribas, Alvaro
   Bouy, Herve
   Bryden, Geoffrey
   Stapelfeldt, Karl
   Padgett, Deborah
TI Herschel/PACS photometry of transiting-planet host stars with candidate
   warm debris disks
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planetary systems; planets and satellites: dynamical evolution and
   stability
ID SUN-LIKE STARS; KEPLER TARGET STARS; SYSTEM; DUST; VEGA; CHARA/FLUOR;
   EVOLUTION; PACS
AB Dust in debris disks is produced by colliding or evaporating planetesimals, which are remnants of the planet formation process. Warm dust disks, known by their emission at <= 24 mu m, are rare (4% of FGK main sequence stars) and especially interesting because they trace material in the region likely to host terrestrial planets, where the dust has a very short dynamical lifetime. Statistical analyses of the source counts of excesses as found with the mid-IR Wide Field Infrared Survey Explorer (WISE) suggest that warm-dust candidates found for the Kepler transiting-planet host-star candidates can be explained by extragalactic or galactic background emission aligned by chance with the target stars. These statistical analyses do not exclude the possibility that a given WISE excess could be due to a transient dust population associated with the target. Here we report Herschel/PACS 100 and 160 micron follow-up observations of a sample of Kepler and non-Kepler transiting-planet candidates' host stars, with candidate WISE warm debris disks, aimed at detecting a possible cold debris disk in any one of them. No clear detections were found in any one of the objects at either wavelength. Our upper limits confirm that most objects in the sample do not have a massive debris disk like that in beta Pic. We also show that the planet-hosting star WASP-33 does not have a debris disk comparable to the one around eta Crv. Although the data cannot be used to rule out rare warm disks around the Kepler planet-hosting candidates, the lack of detections and the characteristics of neighboring emission found at far-IR wavelengths support an earlier result suggesting that most of the WISE-selected IR excesses around Kepler candidate host stars are likely due to either chance alignment with background IR-bright galaxies and/or to interstellar emission.
C1 [Merin, Bruno; Ribas, Alvaro] European Space Astron Ctr ESA, Villanueva De La Canada 28691, Spain.
   [Ardila, David R.] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
   [Ribas, Alvaro; Bouy, Herve] INTA CSIC, Ctr Astrobiol, Villanueva Canada Madrid 28691, Spain.
   [Bryden, Geoffrey] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
   [Stapelfeldt, Karl] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Padgett, Deborah] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Merin, B (reprint author), European Space Astron Ctr ESA, POB 78, Villanueva De La Canada 28691, Spain.
EM bmerin@sciops.esa.int
RI Bouy, Herve/H-2913-2012
OI Bouy, Herve/0000-0002-7084-487X
FU ESAC Trainee Program, ESAC Space Science Faculty; Herschel Science
   Centre; ESA SRE-OA [SC 1300016149]; National Aeronautics and Space
   Administration's Science Mission Directorate (NASA); NASA [NAS5-26555];
   National Science Foundation; Multimission Archive at the Space Telescope
   Science Institute (MAST); NASA Office of Space Science [NNX09AF08G]
FX This work has been possible thanks to the support from the ESAC Trainee
   Program, ESAC Space Science Faculty, and of the Herschel Science Centre.
   AR acknowledges support from the ESA SRE-OA Research Funding via
   contract SC 1300016149. Support for this work was provided by NASA
   through an award issued by JPL/Caltech. This publication is based on
   observations made by the Herschel Space Telescope and the PACS
   instrument. PACS was developed by a consortium of institutes led by MPE
   (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium);
   CEA, LAM (France); MPIA (Germany); INAF-IFSI, OAA, OAP, OAT, LENS, SISSA
   (Italy); IAC (Spain). This development has been supported by the funding
   agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR
   (Germany), ASI, INAF (Italy), and CICYT/MCYT (Spain). HCSS, HSpot and
   HIPE are joint developments by the Herschel Science Ground Segment
   Consortium, consisting of ESA, the NASA Herschel Science Center, and the
   HIFI, PACS and SPIRE consortia. This publication is also based on
   observations made with the Kepler Spacecraft. Funding for this mission
   is provided by National Aeronautics and Space Administration's Science
   Mission Directorate (NASA). This study also makes use of data products
   from Herschel Space Observatory and the Wide- field Infrared Survey
   Explorer, a joint project of the University of California, Los Angeles,
   and the Jet Propulsion Laboratory (JPL)/California Institute of
   Technology (Caltech); the NASA Infrared Processing and Analysis Center
   (IPAC) Science Archive and the NASA/IPAC/NExScI Star and Exoplanet
   Database, operated by JPL, Caltech, and funded by NASA; the SIMBAD
   database and the Vizier service, operated at the Centre de Donnes
   astronomiques de Strasbourg, France; the data products from the Two
   Micron All Sky Survey (2MASS), a joint project of the University of
   Massachusetts and IPAC at Caltech, funded by NASA and the National
   Science Foundation; the Multimission Archive at the Space Telescope
   Science Institute (MAST). STScI is operated by the Association of
   Universities for Research in Astronomy, Inc., under NASA contract
   NAS5-26555. Support for MAST for non-HST data is provided by the NASA
   Office of Space Science via grant NNX09AF08G and by other grants and
   contracts.
NR 36
TC 0
Z9 0
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
   FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2014
VL 569
AR A89
DI 10.1051/0004-6361/201322956
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8PZ
UT WOS:000343092100023
ER

PT J
AU Muller, C
   Kadler, M
   Ojha, R
   Perucho, M
   Grossberger, C
   Ros, E
   Wilms, J
   Blanchard, J
   Bock, M
   Carpenter, B
   Dutka, M
   Edwards, PG
   Hase, H
   Horiuchi, S
   Kreikenbohm, A
   Lovell, JEJ
   Markowitz, A
   Phillips, C
   Plotz, C
   Pursimo, T
   Quick, J
   Rothschild, R
   Schulz, R
   Steinbring, T
   Stevens, J
   Trustedt, J
   Tzioumis, AK
AF Mueller, C.
   Kadler, M.
   Ojha, R.
   Perucho, M.
   Grossberger, C.
   Ros, E.
   Wilms, J.
   Blanchard, J.
   Boeck, M.
   Carpenter, B.
   Dutka, M.
   Edwards, P. G.
   Hase, H.
   Horiuchi, S.
   Kreikenbohm, A.
   Lovell, J. E. J.
   Markowitz, A.
   Phillips, C.
   Ploetz, C.
   Pursimo, T.
   Quick, J.
   Rothschild, R.
   Schulz, R.
   Steinbring, T.
   Stevens, J.
   Truestedt, J.
   Tzioumis, A. K.
TI TANAMI monitoring of Centaurus A: The complex dynamics in the inner
   parsec of an extragalactic jet
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: individual: Centaurus A; galaxies:
   individual: NGC 5128; techniques: high angular resolution; galaxies:
   jets
ID ACTIVE GALACTIC NUCLEI; SUBPARSEC-SCALE STRUCTURE; SUPERMASSIVE
   BLACK-HOLE; LINE ARRAY OBSERVATIONS; EGRET-DETECTED QUASARS; RECENT
   STAR-FORMATION; BL LACERTAE OBJECTS; GAMMA-RAY EMISSION; X-RAY; RADIO
   JETS
AB Context. Centaurus A (Cen A) is the closest radio-loud active galactic nucleus. Very Long Baseline Interferometry (VLBI) enables us to study the spectral and kinematic behavior of the radio jet-counterjet system on milliarcsecond scales, providing essential information for jet emission and propagation models.
   Aims. In the framework of the TANAMI monitoring, we investigate the kinematics and complex structure of Cen A on subparsec scales. We have been studying the evolution of the central parsec jet structure of CenA for over 3.5 years. The proper motion analysis of individual jet components allows us to constrain jet formation and propagation and to test the proposed correlation of increased high-energy flux with jet ejection events. Cen A is an exceptional laboratory for such a detailed study because its proximity translates to unrivaled linear resolution, where one milliarcsecond corresponds to 0.018 pc.
   Methods. As a target of the southern-hemisphere VLBI monitoring program TANAMI, observations of CenA are done approximately every six months at 8.4 GHz with the Australian Long Baseline Array (LBA) and associated telescopes in Antarctica, Chile, New Zealand, and South Africa, complemented by quasi-simultaneous 22.3 GHz observations.
   Results. The first seven epochs of high-resolution TANAMI VLBI observations at 8.4 GHz of CenA are presented, resolving the jet on (sub-) milliarcsecond scales. They show a differential motion of the subparsec scale jet with significantly higher component speeds farther downstream where the jet becomes optically thin. We determined apparent component speeds within a range of 0 : 1 c to 0 : 3 c and identified long-term stable features. In combination with the jet-to-counterjet ratio, we can constrain the angle to the line of sight to theta similar to 12 degrees-45 degrees.
   Conclusions. The high-resolution kinematics are best explained by a spine-sheath structure supported by the downstream acceleration occurring where the jet becomes optically thin. On top of the underlying, continuous flow, TANAMI observations clearly resolve individual jet features. The flow appears to be interrupted by an obstacle causing a local decrease in surface brightness and circumfluent jet behavior. We propose a jet-star interaction scenario to explain this appearance. The comparison of jet ejection times to high X-ray flux phases yields a partial overlap of the onset of the X-ray emission and increasing jet activity, but the limited data do not support a robust correlation.
C1 [Mueller, C.; Grossberger, C.; Wilms, J.; Kreikenbohm, A.; Markowitz, A.; Schulz, R.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany.
   [Mueller, C.; Kadler, M.; Grossberger, C.; Kreikenbohm, A.; Schulz, R.; Steinbring, T.; Truestedt, J.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
   [Ojha, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
   [Ojha, R.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
   [Ojha, R.; Carpenter, B.; Dutka, M.] Catholic Univ Amer, Washington, DC 20064 USA.
   [Perucho, M.; Ros, E.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
   [Ros, E.; Boeck, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
   [Ros, E.] Univ Valencia, Astron Observ, Valencia 46980, Spain.
   [Blanchard, J.] Univ Concepcion, Dept Astron, Concepcion, Chile.
   [Edwards, P. G.; Phillips, C.; Stevens, J.; Tzioumis, A. K.] CSIRO Astron & Space Sci, ATNF, Epping, NSW 1710, Australia.
   [Hase, H.; Ploetz, C.] Bundesamt Kartog & Geodasie, D-93444 Bad Kotzting, Germany.
   [Horiuchi, S.] CSIRO Astron & Space Sci, Tuggeranong, ACT 2901, Australia.
   [Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
   [Markowitz, A.; Rothschild, R.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
   [Pursimo, T.] Nord Opt Telescope Apartado, Santa Cruz Palma Palma S 38700, Spain.
   [Quick, J.] Hartebeesthoek Radio Astron Observ, Krugersdorp, South Africa.
RP Muller, C (reprint author), Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, Sternwartstr 7, D-96049 Bamberg, Germany.
EM cornelia.mueller@sternwarte.uni-erlangen.de
RI Wilms, Joern/C-8116-2013; Perucho, Manel/A-9528-2017; 
OI Wilms, Joern/0000-0003-2065-5410; Perucho, Manel/0000-0003-2784-0379;
   Ros, Eduardo/0000-0001-9503-4892; Kadler, Matthias/0000-0001-5606-6154
FU Studienstiftung des Deutschen Volkes; Spanish MINECO
   [AYA2009-13036-C02-02, AYA2012-38491-C02-01]; Generalitat Valenciana
   [PROMETEO/2009/104]; COST action "Black Holes in a Violent Universe"
   [MP0905]; Spanish "Ministerio de Ciencia e Innovacion" (MICINN)
   [AYA2010-21322-C03-01, AYA2010-21097-C03-01]; Universitat de Valencia;
   Max-Planck-Institut fur Radioastronomie; Commonwealth of Australia; NASA
   [NNH09ZDA001N, NNH10ZDA001N, NNH12ZDA001N]; National Aeronautics and
   Space Administration
FX The authors acknowledge the helpful discussions and suggestions by A.
   Lobanov and K. Mannheim, and especially thank the anonymous referee for
   valuable comments that improved the paper. C.M. acknowledges the support
   by the "Studienstiftung des Deutschen Volkes". E.R. was partially
   supported by the Spanish MINECO projects AYA2009-13036-C02-02 and
   AYA2012-38491-C02-01 and by the Generalitat Valenciana project
   PROMETEO/2009/104, as well as by the COST MP0905 action "Black Holes in
   a Violent Universe". M.P. acknowledges financial support by the Spanish
   "Ministerio de Ciencia e Innovacion" (MICINN) grants
   AYA2010-21322-C03-01, AYA2010-21097-C03-01, and support by Universitat
   de Valencia and Max-Planck-Institut fur Radioastronomie. The Australian
   Long Baseline Array is part of the Australia Telescope National
   Facility, which is funded by the Commonwealth of Australia for operation
   as a National Facility managed by CSIRO. This research was funded in
   part by NASA through Fermi Guest Investigator grants NNH09ZDA001N,
   NNH10ZDA001N, and NNH12ZDA001N. 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. This research made use of data from 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; and the SIMBAD database (operated
   at the CDS, Strasbourg, France).
NR 93
TC 14
Z9 14
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
   FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2014
VL 569
AR A115
DI 10.1051/0004-6361/201423948
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8PZ
UT WOS:000343092100078
ER

PT J
AU Sanchez-Monge, A
   Beltran, MT
   Cesaroni, R
   Etoka, S
   Galli, D
   Kumar, MSN
   Moscadelli, L
   Stanke, T
   van der Tak, FFS
   Vig, S
   Walmsley, CM
   Wang, KS
   Zinnecker, H
   Elia, D
   Molinari, S
   Schisano, E
AF Sanchez-Monge, A.
   Beltran, M. T.
   Cesaroni, R.
   Etoka, S.
   Galli, D.
   Kumar, M. S. N.
   Moscadelli, L.
   Stanke, T.
   van der Tak, F. F. S.
   Vig, S.
   Walmsley, C. M.
   Wang, K. -S.
   Zinnecker, H.
   Elia, D.
   Molinari, S.
   Schisano, E.
TI A necklace of dense cores in the high-mass star forming region
   G35.20-0.74 N: ALMA observations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; stars: massive; ISM: individual objects: G35.20-0.74
   N; ISM: molecules; ISM: jets and outflows
ID YOUNG STELLAR OBJECTS; GRAIN-SURFACE-CHEMISTRY; MOLECULAR LINE SURVEY;
   GHZ METHANOL MASERS; HOT-CORE; MAGNETIC-FIELD; ORION-KL; MIDINFRARED
   INTERFEROMETRY; HIERARCHICAL FRAGMENTATION; INTERSTELLAR JETS
AB Context. The formation process of high-mass stars (with masses >8 M-circle dot) is still poorly understood, and represents a challenge from both the theoretical and observational points of view. The advent of the Atacama Large Millimeter Array (ALMA) is expected to provide observational evidence to better constrain the theoretical scenarios.
   Aims. The present study aims at characterizing the high-mass star forming region G35.20-0.74 N, which is found associated with at least one massive outflow and contains multiple dense cores, one of them recently found associated with a Keplerian rotating disk.
   Methods. We used the radio-interferometer ALMA to observe the G35.20-0.74 N region in the submillimeter continuum and line emission at 350 GHz. The observed frequency range covers tracers of dense gas (e.g., (HCO+)-C-13, (CO)-O-17), molecular outflows (e.g., SiO), and hot cores (e.g., CH3CN, CH3OH). These observations were complemented with infrared and centimeter data.
   Results. The ALMA 870 mu m continuum emission map reveals an elongated dust structure (similar to 0.15 pc long and similar to 0.013 pc wide; full width at half maximum) perpendicular to the large-scale molecular outflow detected in the region, and fragmented into a number of cores with masses similar to 1-10 M-circle dot and sizes similar to 1600 AU (spatial resolution similar to 960 AU). The cores appear regularly spaced with a separation of similar to 0.023 pc. The emission of dense gas tracers such as (HCO+)-C-13 or (CO)-O-17 is extended and coincident with the dust elongated structure. The three strongest dust cores show emission of complex organic molecules characteristic of hot cores, with temperatures around 200 K, and relative abundances 0.2-2 x 10(-8) for CH3CN and 0.6-5 x 10(-6) for CH3OH. The two cores with highest mass (cores A and B) show coherent velocity fields, with gradients almost aligned with the dust elongated structure. Those velocity gradients are consistent with Keplerian disks rotating about central masses of 4-18 M-circle dot. Perpendicular to the velocity gradients we have identified a large-scale precessing jet/outflow associated with core B, and hints of an east-west jet/outflow associated with core A.
   Conclusions. The elongated dust structure in G35.20-0.74 N is fragmented into a number of dense cores that may form high-mass stars. Based on the velocity field of the dense gas, the orientation of the magnetic field, and the regularly spaced fragmentation, we interpret this elongated structure as the densest part of a 1D filament fragmenting and forming high-mass stars.
C1 [Sanchez-Monge, A.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
   [Sanchez-Monge, A.; Beltran, M. T.; Cesaroni, R.; Galli, D.; Moscadelli, L.; Walmsley, C. M.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
   [Etoka, S.] Hamburger Sternwarte, D-21029 Hamburg, Germany.
   [Etoka, S.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
   [Kumar, M. S. N.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
   [Stanke, T.] ESO, D-85748 Garching, Germany.
   [van der Tak, F. F. S.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands.
   [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
   [Vig, S.] Indian Inst Space Sci & Technol, Dept Earth & Space Sci, Thiruvananthapuram 695547, Kerala, India.
   [Walmsley, C. M.] DIAS, Dublin 2, Ireland.
   [Wang, K. -S.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
   [Zinnecker, H.] NASA, SOFIA Sci Ctr, Ames Res Ctr, Moffett Field, CA 94035 USA.
   [Elia, D.; Molinari, S.] INAF, IAPS, I-00133 Rome, Italy.
   [Schisano, E.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
RP Sanchez-Monge, A (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany.
EM sanchez@ph1.uni-koeln.de
RI Molinari, Sergio/O-4095-2016; 
OI Molinari, Sergio/0000-0002-9826-7525; Cesaroni,
   Riccardo/0000-0002-2430-5103; Beltran Sorolla, Maria
   Teresa/0000-0003-3315-5626; Moscadelli, Luca/0000-0002-8517-8881; Galli,
   Daniele/0000-0001-7706-6049; Elia, Davide/0000-0002-9120-5890
FU National Aeronautics and Space Administration
FX We are grateful to the Italian ARC node for the usage of their computer
   facilities during the cleaning and imaging process. We are also grateful
   to Ray Furuya for providing us the ASTE spectrum, and to Keping Qiu for
   providing the SMA spectra. A.S.-M. is grateful to Peter Schilke, Thomas
   Moller and Alexander Zernickel for helping with the analysis of the
   myXCLASS software. This paper makes use of the following ALMA data:
   ADS/JAO.ALMA#2011.0.00275.S. ALMA is a partnership of ESO (representing
   its member states), NSF (USA) and NINS (Japan), together with NRC
   (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of
   Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ.
   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.
NR 93
TC 11
Z9 11
U1 1
U2 7
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
   FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2014
VL 569
AR A11
DI 10.1051/0004-6361/201424032
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8PZ
UT WOS:000343092100086
ER

PT J
AU Schmieder, B
   Tian, H
   Kucera, T
   Ariste, AL
   Mein, N
   Mein, P
   Dalmasse, K
   Golub, L
AF Schmieder, B.
   Tian, H.
   Kucera, T.
   Lopez Ariste, A.
   Mein, N.
   Mein, P.
   Dalmasse, K.
   Golub, L.
TI Open questions on prominences from coordinated observations by IRIS,
   Hinode, SDO/AIA, THEMIS, and the Meudon/MSDP
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: magnetic fields; Sun: filaments, prominences; Sun: transition
   region
ID SOLAR OPTICAL TELESCOPE; MAGNETIC-FIELD VECTOR; QUIESCENT PROMINENCES;
   FILAMENT CHANNEL; RADIATIVE-TRANSFER; ACTIVE-REGION; LINES; SOHO/SUMER;
   POLARIZATION; EMERGENCE
AB Context. A large prominence was observed by multiple instruments on the ground and in space during an international campaign on September 24, 2013, for three hours (12: 12 UT -15: 12 UT). Instruments used in the campaign included the newly launched (June 2013) Interface Region Imaging Spectrograph (IRIS), THEMIS (Tenerife), the Hinode Solar Optical Telescope (SOT), the Solar Dynamic Observatory's Atmospheric Imaging Assembly (SDO/AIA), and the Multichannel Subtractive Double Pass spectrograph (MSDP) in the Meudon Solar Tower. The movies obtained in 304 angstrom with the EUV imager SDO/AIA, and in Ca II line by SOT show the dynamic nature of the prominence.
   Aims. The aim of this work is to study the dynamics of the prominence fine structures in multiple wavelengths to understand their formation.
   Methods. The spectrographs IRIS and MSDP provided line profiles with a high cadence in Mg II h (2803.5 angstrom) and k (2796.4 angstrom) lines along four slit positions (IRIS), and in Ha in a 2D field of view (MSDP). The spectropolarimetry of THEMIS (Tenerife) allowed us to derive the magnetic field of the prominence using the He D-3 line depolarization (Hanle effect combined with the Zeeman effect).
   Results. The magnetic field is found to be globally horizontal with a relatively weak field strength (8-15 Gauss). On the other hand, the Ca II movie reveals turbulent-like motion that is not organized in specific parts of the prominence. We tested the addition of a turbulent magnetic component. This model is compatible with the polarimetric observations at those places where the plasma turbulence peaks. On the other hand, the Mg II line profiles show multiple peaks well separated in wavelength. This is interpreted by the existence of small threads along the line of sight with a large dispersion of discrete values of Doppler shifts, from 5 km s(-1) (a quasi-steady component) to 60-80 km s(-1). Each peak corresponds to a Gaussian profile, and not to a reversed profile as was expected by the present non-LTE radiative transfer modeling. This is a very surprising behavior for the Mg II line observed in prominences.
   Conclusions. Turbulent fields on top of the macroscopic horizontal component of the magnetic field supporting the prominence give rise to the complex dynamics of the plasma. The plasma with the high velocities (70 km s(-1) to 100 km s(-1) if we take into account the transverse velocities) may correspond to condensation of plasma along more or less horizontal threads of the arch-shape structure visible in 304 angstrom. The steady flows (5 km s(-1)) would correspond to a more quiescent plasma (cool and prominence-corona transition region) of the prominence packed into dips in horizontal magnetic field lines. The very weak secondary peaks in the Mg II profiles may reflect the turbulent nature of parts of the prominence.
C1 [Schmieder, B.; Mein, N.; Mein, P.; Dalmasse, K.] Observ Paris, LESIA, Sect Meudon, F-75014 Paris, France.
   [Tian, H.; Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
   [Kucera, T.] NASA, Gsfc, MD USA.
   [Lopez Ariste, A.] CNRS, THEMIS, Tenerife 38200, Spain.
RP Schmieder, B (reprint author), Observ Paris, LESIA, Sect Meudon, F-75014 Paris, France.
EM brigitte.schmieder@obspm.fr
OI Kucera, Therese/0000-0001-9632-447X
FU Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract;
   NASA's LWS program; LMSAL [8100002705]
FX IRIS is a NASA small explorer mission developed and operated by LMSAL
   with mission operations executed at NASA Ames Research center and major
   contributions to downlink communications funded by the Norwegian Space
   Center (NSC, Norway) through an ESA PRODEX contract. Hinode is a
   Japanese mission developed and launched by ISAS/JAXA, with NAOJ as
   domestic partner and NASA and STFC (UK) as international partners. It is
   operated by these agencies in co-operation with ESA and NSC (Norway).
   SDO data are courtesy of NASA/SDO and the AIA science team. T.K. thanks
   NASA's LWS program for support. We thank also the team of THEMIS and
   particularly B. Gelly, the director of THEMIS allowing us to obtain
   coordinated observations of this prominence. We would like to thank D.
   Shine for providing the HINODE/SOT data, D.Crussaire, and R. Le Cocguen
   for the observations in the solar tower in Meudon. We thank deeply Peter
   Martens and Petr Heinzel for their fruitful comments which help us to
   improve the manuscript. H.T. is supported by contract 8100002705 from
   LMSAL to SAO.
NR 51
TC 14
Z9 14
U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
   FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2014
VL 569
AR A85
DI 10.1051/0004-6361/201423922
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8PZ
UT WOS:000343092100075
ER

PT J
AU Thirouin, A
   Noll, KS
   Ortiz, JL
   Morales, N
AF Thirouin, A.
   Noll, K. S.
   Ortiz, J. L.
   Morales, N.
TI Rotational properties of the binary and non-binary populations in the
   trans-Neptunian belt
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planetary systems; Kuiper belt: general; techniques: photometric
ID SHORT-TERM VARIABILITY; NEAR-EARTH ASTEROIDS; DEEP ECLIPTIC SURVEY;
   42355 TYPHON-ECHIDNA; PLANET 136199 ERIS; KUIPER-BELT; HERSCHEL-PACS;
   LIGHT CURVES; 90482 ORCUS; 2003 EL61
AB We present results for the short-term variability of binary trans-Neptunian objects (BTNOs). We performed CCD photometric observations using the 3.58 m Telescopio Nazionale Galileo (TNG), the 1.5 m Sierra Nevada Observatory (OSN) telescope, and the 1.23 m Centro Astronomico Hispano Aleman (CAHA) telescope at Calar Alto Observatory. We present results based on five years of observations and report the short-term variability of six BTNOs. Our sample contains three classical objects: (174567) 2003 MW12, or Varda, (120347) 2004 SB60, or Salacia, and 2002 VT130; one detached disk object: (229762) 2007 UK126; and two resonant objects: (341520) 2007 TY430 and (38628) 2000 EB173, or Huya. For each target, possible rotational periods and/or photometric amplitudes are reported. We also derived some physical properties from their light curves, such as density, primary and secondary sizes, and albedo. We compiled and analyzed a vast light curve database for TNOs including centaurs to determine the light-curve amplitude and spin frequency distributions for the binary and non-binary populations. The mean rotational periods, from the Maxwellian fits to the frequency distributions, are 8.63 +/- 0.52 h for the entire sample, 8.37 +/- 0.58 h for the sample without the binary population, and 10.11 +/- 1.19 h for the binary population alone. Because the centaurs are collisionally more evolved, their rotational periods might not be so primordial. We computed a mean rotational period, from the Maxwellian fit, of 8.86 +/- 0.58 h for the sample without the centaur population, and of 8.64 +/- 0.67 h considering a sample without the binary and the centaur populations. According to this analysis, regular TNOs spin faster than binaries, which is compatible with the tidal interaction of the binaries. Finally, we examined possible formation models for several systems studied in this work and by our team in previous papers.
C1 [Thirouin, A.; Ortiz, J. L.; Morales, N.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
   [Thirouin, A.; Noll, K. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Thirouin, A (reprint author), CSIC, Inst Astrofis Andalucia, Apt 3004, E-18080 Granada, Spain.
EM thirouin@iaa.es
FU Spanish MICINN/MEC projects [AYA2008-06202-C03-01, AYA2011-30106-C02-01]
FX We thank the referee for his or her careful reading of this paper. We
   are grateful to the Sierra Nevada Observatory, Telescopio Nazionale
   Galileo and CAHA staffs. This research was based on data obtained at the
   Observatorio de Sierra Nevada, which is operated by the Instituto de
   Astrofisica de Andalucia, CSIC. Other results were obtained at the
   Telescopio Nazionale Galileo. The Telescopio Nazionale Galileo (TNG) is
   operated by the Fundacion Galileo Galilei of the Italian Istituto
   Nazionale di Astrofisica (INAF) on the island of La Palma in the Spanish
   Observatorio del Roque de los Muchachos of the Instituto de Astrofisica
   de Canarias. This research is also based on observations collected at
   the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, operated
   jointly by the Max-Planck Institut fur Astronomie and the Instituto de
   Astrofisica de Andalucia (CSIC). A. Thirouin, N. Morales, and J. L.
   Ortiz were supported by AYA2008-06202-C03-01, and AYA2011-30106-C02-01,
   which are two Spanish MICINN/MEC projects. A. Thirouin, N. Morales, and
   J. L. Ortiz also acknowledge the Proyecto de Excelencia de la Junta de
   Andalucia, J.A.2007-FQM2998. FEDER funds are also acknowledged.
NR 108
TC 4
Z9 4
U1 0
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
   FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2014
VL 569
AR A3
DI 10.1051/0004-6361/201423567
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8PZ
UT WOS:000343092100051
ER

PT J
AU Urrutia-Viscarra, F
   Arnaboldi, M
   de Oliveira, CM
   Gerhard, O
   Torres-Flores, S
   Carrasco, ER
   de Mello, D
AF Urrutia-Viscarra, F.
   Arnaboldi, M.
   Mendes de Oliveira, C.
   Gerhard, O.
   Torres-Flores, S.
   Carrasco, E. R.
   de Mello, D.
TI A census of Ha emitters in the intergalactic medium of the NGC 2865
   system
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: abundances; HII regions; galaxies: individual: NGC 2865; galaxies:
   dwarf; galaxies: ISM; galaxies: star formation
ID INTRACLUSTER PLANETARY-NEBULAE; TIDAL DWARF GALAXIES; STAR-FORMING
   GALAXIES; CIV MASS DENSITY; VIRGO CLUSTER; COMA CLUSTER; IRREGULAR
   GALAXIES; EVOLUTION-EXPLORER; ELLIPTIC GALAXIES; STEPHANS-QUINTET
AB Tidal debris, which are rich in HI gas and formed in interacting and merging systems, are suitable laboratories to study star formation outside galaxies. Recently, several such systems were observed, which contained many young star forming regions outside the galaxies. In previous works, we have studied young star forming regions outside galaxies in different systems with optical and/or gaseous tidal debris, in order to understand how often they occur and in which type of environments. In this paper, we searched for star forming regions around the galaxy NGC 2865, a shell galaxy that is circled by a ring of HI with a total mass of 1.2x10(9) M-circle dot. Using the multi-slit imaging spectroscopy technique with the Gemini telescope, we detected all H alpha emitting sources in the surroundings of the galaxy NGC 2865, down to a flux limit of 10(-18) erg cm(-2) s(-1) angstrom(-1). With the spectra information and the near and far-ultraviolet flux, we characterize the star formation rates, masses, ages, and metallicities for these HII regions. In total, we found 26 emission-line sources in a 60 x 60 Kpc field centered over the southeastern tail of the HI gas present around the galaxy NGC 2865. Out of the 26 Ha emitters, 19 are in the satellite galaxy FGCE 0745, and seven are intergalactic HII regions scattered over the south tail of the HI gas around NGC 2865. We found that the intergalactic HII regions are young (<200 Myr) with stellar masses in the range 4 x 10(3) M-circle dot to 17 x 10(6) M-circle dot. These are found in a region of low HI gas density, where the probability of forming stars is expected to be low. For one of the intergalactic HII regions, we estimated a solar oxygen abundance of 12 + log(O/H) similar to 8.7. We also were able to estimate the metallicity for the satellite galaxy FGCE 0745 to be 12 + log(O/H) similar to 8.0. Given these physical parameters, the intergalactic HII regions are consistent with young star forming regions (or clusters), which are born in situ outside the NGC 2865 galaxy from a pre-enriched gas removed from the host galaxies in a merger event. The relevance of these observations is discussed.
C1 [Urrutia-Viscarra, F.; Arnaboldi, M.] European So Observ, D-85748 Garching, Germany.
   [Urrutia-Viscarra, F.; Mendes de Oliveira, C.] Univ Sao Paulo, Inst Astron Geofins Ciencias & Atmosfer, BR-05508900 Sao Paulo, Brazil.
   [Gerhard, O.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
   [Torres-Flores, S.] Univ La Serena, Dept Fis, La Serena, Chile.
   [Carrasco, E. R.] Gemini Observ AURA, Southern Operat Ctr, La Serena, Chile.
   [de Mello, D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
   [de Mello, D.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
RP Urrutia-Viscarra, F (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM furrutia@astro.iag.usp.br
RI Mendes de Oliveira, Claudia/F-2391-2012
OI Mendes de Oliveira, Claudia/0000-0002-7736-4297
FU ESO; CNPq; FAPESP [2006/56213-9]; Chilean agency FONDECYT [11121505];
   NASA ADAP [NNX09AC72G];  [CONICYT PAI/ACADEMIA 7912010004]
FX The authors would like to thank the anonymous referee for the thoughtful
   comments which improved the clarity of this paper. We would like to
   thank C. D. P. Lagos, L. Coccato and A. Longobardi for help and useful
   discussions. This work is based on observation obtained with the Gemini
   telescope. This work has made used of NED-database, Mikulski Archive for
   Space Telescope (MAST). F.U.-V. acknowledges the financial support of
   ESO studentship programme and CNPq through a Ph.D. CMdO thanks FAPESP
   for funding through thematic grant 2006/56213-9. S.T.-F. acknowledges
   the financial support of the Chilean agency FONDECYT through a project
   "Iniciacion en la Investigacion", under contract 11121505 and S.T.-F.
   also acknowledges the support of the project CONICYT PAI/ACADEMIA
   7912010004. DFdM was partially funded by NASA ADAP NNX09AC72G.
NR 65
TC 1
Z9 1
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
   FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2014
VL 569
AR A97
DI 10.1051/0004-6361/201323025
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA AQ8PZ
UT WOS:000343092100025
ER

PT J
AU Hartwig, J
   Mann, JA
   Darr, SR
AF Hartwig, Jason
   Mann, Jay Adin, Jr.
   Darr, Samuel R.
TI Parametric analysis of the liquid hydrogen and nitrogen bubble point
   pressure for cryogenic liquid acquisition devices
SO CRYOGENICS
LA English
DT Article
DE Liquid acquisition devices; Liquid hydrogen; Liquid nitrogen; Porous
   screen; Bubble point; Fuel depot; Pressurant gas
ID SCREEN; TESTS
AB This paper presents the parametric investigation of the factors which govern screen channel liquid acquisition device bubble point pressure in a low pressure propellant tank. The five test parameters that were varied included the screen mesh, liquid cryogen, liquid temperature and pressure, and type of pressurant gas. Bubble point data was collected using three fine mesh 304 stainless steel screens in two different liquids (hydrogen and nitrogen), over a broad range of liquid temperatures and pressures in subcooled and saturated liquid states, using both a noncondensible (helium) and autogenous (hydrogen or nitrogen) gas pressurization scheme. Bubble point pressure scales linearly with surface tension, but does not scale inversely with the fineness of the mesh. Bubble point pressure increases proportional to the degree of subcooling. Higher bubble points are obtained using noncondensible pressurant gases over the condensable vapor. The bubble point model is refined using a temperature dependent pore diameter of the screen to account for screen shrinkage at reduced liquid temperatures and to account for relative differences in performance between the two pressurization schemes. The updated bubble point model can be used to accurately predict performance of LADs operating in future cryogenic propellant engines and cryogenic fuel depots. Published by Elsevier Ltd.
C1 [Hartwig, Jason] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
   [Mann, Jay Adin, Jr.] Case Western Reserve Univ, Cleveland, OH 44106 USA.
   [Darr, Samuel R.] Univ Florida, Gainesville, FL 32611 USA.
RP Hartwig, J (reprint author), NASA, Glenn Res Ctr, M-S 301-3,, Cleveland, OH 44135 USA.
EM Jason.W.Hartwig@nasa.gov
NR 40
TC 9
Z9 10
U1 0
U2 6
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-OCT
PY 2014
VL 63
BP 25
EP 36
DI 10.1016/j.cryogenics.2014.05.013
PG 12
WC Thermodynamics; Physics, Applied
SC Thermodynamics; Physics
GA AR6IF
UT WOS:000343686700003
ER

PT J
AU Phillips, AJ
   Ciannelli, L
   Brodeur, RD
   Pearcy, WG
   Childers, J
AF Phillips, A. Jason
   Ciannelli, Lorenzo
   Brodeur, Richard D.
   Pearcy, William G.
   Childers, John
TI Spatio-temporal associations of albacore CPUEs in the Northeastern
   Pacific with regional SST and climate environmental variables
SO ICES JOURNAL OF MARINE SCIENCE
LA English
DT Article
DE albacore; environmental variables; regime shifts; spatial distribution;
   temporal distribution
ID CALIFORNIA CURRENT SYSTEM; SEA-SURFACE TEMPERATURE; THUNNUS-ALALUNGA;
   NORTH PACIFIC; INTERDECADAL VARIABILITY; OCEANOGRAPHIC CONDITIONS;
   SPATIAL-DISTRIBUTION; DECADAL OSCILLATION; FISH POPULATION; OCEAN
AB This study investigated the spatial distribution of juvenile North Pacific albacore (Thunnus alalunga) in relation to local environmental variability [i.e. sea surface temperature (SST)], and two large-scale indices of climate variability, [the Pacific Decadal Oscillation (PDO) and the Multivariate El Nino/Southern Oscillation Index (MEI)]. Changes in local and climate variables were correlated with 48 years of albacore troll catch per unit effort (CPUE) in 1 degrees latitude/longitude cells, using threshold Generalized Additive Mixed Models (tGAMMs). Model terms were included to account for non-stationary and spatially variable effects of the intervening covariates on albacore CPUE. Results indicate that SST had a positive and spatially variable effect on albacore CPUE, with increasingly positive effects to the North, while PDO had an overall negative effect. Although albacore CPUE increased with SST both before and after a threshold year of 1986, such effect geographically shifted north after 1986. This is the first study to demonstrate the non-stationary spatial dynamics of albacore tuna, linked with a major shift of the North Pacific. Results imply that if ocean temperatures continue to increase, US west coast fisher communities reliant on commercial albacore fisheries are likely to be negatively affected in the southern areas but positively affected in the northern areas, where current albacore landings are highest.
C1 [Phillips, A. Jason; Ciannelli, Lorenzo; Pearcy, William G.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
   [Brodeur, Richard D.] Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Newport, OR 97365 USA.
   [Childers, John] Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, La Jolla, CA 92037 USA.
RP Phillips, AJ (reprint author), Oregon State Univ, Coll Earth Ocean & Atmospher Sci, 104 CEOAS Adm Bldg, Corvallis, OR 97331 USA.
EM ajasonphillips@gmail.com
FU Oregon Sea Grant under National Oceanic and Atmospheric Administration's
   National Sea Grant College Program, U.S. Department of Commerce
   [NA06OAR4170010, R/RCF-25]; NWFSC; SWFSC
FX This report was prepared by Oregon Sea Grant under grant number
   NA06OAR4170010 (project number R/RCF-25) from the National Oceanic and
   Atmospheric Administration's National Sea Grant College Program, U.S.
   Department of Commerce, and by appropriations made by the Oregon State
   Legislature. The statements, findings, conclusions, and recommendations
   are those of the authors and do not necessarily reflect the views of
   these funders. We would also like to acknowledge that Richard Brodeur
   was supported by funding provided by the NWFSC and John Childers and the
   collection of albacore data were supported by funding provided by the
   SWFSC.
NR 60
TC 2
Z9 2
U1 4
U2 27
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 1054-3139
EI 1095-9289
J9 ICES J MAR SCI
JI ICES J. Mar. Sci.
PD SEP-OCT
PY 2014
VL 71
IS 7
BP 1717
EP 1727
DI 10.1093/icesjms/fst238
PG 11
WC Fisheries; Marine & Freshwater Biology; Oceanography
SC Fisheries; Marine & Freshwater Biology; Oceanography
GA AR1BT
UT WOS:000343315900018
ER

PT J
AU Nachon, M
   Clegg, SM
   Mangold, N
   Schroder, S
   Kah, LC
   Dromart, G
   Ollila, A
   Johnson, JR
   Oehler, DZ
   Bridges, JC
   Le Mouelic, S
   Forni, O
   Wiens, RC
   Anderson, RB
   Blaney, DL
   Bell, JF
   Clark, B
   Cousin, A
   Dyar, MD
   Ehlmann, B
   Fabre, C
   Gasnault, O
   Grotzinger, J
   Lasue, J
   Lewin, E
   Leveille, R
   McLennan, S
   Maurice, S
   Meslin, PY
   Rapin, W
   Rice, M
   Squyres, SW
   Stack, K
   Sumner, DY
   Vaniman, D
   Wellington, D
AF Nachon, M.
   Clegg, S. M.
   Mangold, N.
   Schroeder, S.
   Kah, L. C.
   Dromart, G.
   Ollila, A.
   Johnson, J. R.
   Oehler, D. Z.
   Bridges, J. C.
   Le Mouelic, S.
   Forni, O.
   Wiens, R. C.
   Anderson, R. B.
   Blaney, D. L.
   Bell, J. F.
   Clark, B.
   Cousin, A.
   Dyar, M. D.
   Ehlmann, B.
   Fabre, C.
   Gasnault, O.
   Grotzinger, J.
   Lasue, J.
   Lewin, E.
   Leveille, R.
   McLennan, S.
   Maurice, S.
   Meslin, P. -Y.
   Rapin, W.
   Rice, M.
   Squyres, S. W.
   Stack, K.
   Sumner, D. Y.
   Vaniman, D.
   Wellington, D.
TI Calcium sulfate veins characterized by ChemCam/Curiosity at Gale crater,
   Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars; Curiosity; ChemCam; sulfates; alteration; LIBS
ID INDUCED BREAKDOWN SPECTROSCOPY; CHEMCAM INSTRUMENT SUITE; OMEGA/MARS
   EXPRESS; GYPSUM; STRONTIUM; ROVER; GEOCHEMISTRY; EVAPORITES; CHLORINE;
   BASINS
AB The Curiosity rover has analyzed abundant light-toned fracture-fill material within the Yellowknife Bay sedimentary deposits. The ChemCam instrument, coupled with Mastcam and ChemCam/Remote Micro Imager images, was able to demonstrate that these fracture fills consist of calcium sulfate veins, many of which appear to be hydrated at a level expected for gypsum and bassanite. Anhydrite is locally present and is found in a location characterized by a nodular texture. An intricate assemblage of veins crosses the sediments, which were likely formed by precipitation from fluids circulating through fractures. The presence of veins throughout the entire similar to 5 m thick Yellowknife Bay sediments suggests that this process occurred well after sedimentation and cementation/lithification of those sediments. The sulfur-rich fluids may have originated in previously precipitated sulfate-rich layers, either before the deposition of the Sheepbed mudstones or from unrelated units such as the sulfates at the base of Mount Sharp. The occurrence of these veins after the episodes of deposition of fluvial sediments at the surface suggests persistent aqueous activity in relatively nonacidic conditions.
C1 [Nachon, M.; Mangold, N.; Le Mouelic, S.] Univ Nantes, CNRS, Laboratoire Planetol & Geodynam Nantes, UMR6112, Nantes, France.
   [Clegg, S. M.; Wiens, R. C.; Cousin, A.] Alamos Natl Lab, Los Alamos, NM USA.
   [Schroeder, S.; Forni, O.; Gasnault, O.; Lasue, J.; Maurice, S.; Meslin, P. -Y.; Rapin, W.] Inst Rech Astrophys & Planetol, Toulouse, France.
   [Kah, L. C.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA.
   [Dromart, G.] Univ Lyon, Lab Geol Lyon, Lyon, France.
   [Ollila, A.] Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM USA.
   [Johnson, J. R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
   [Oehler, D. Z.] Jacobs Technology Inc, Johnson Space Ctr, Houston, TX USA.
   [Bridges, J. C.] Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester, Leics, England.
   [Anderson, R. B.] Astrogeol Sci Ctr, S Geol Survey, Flagstaff, AZ USA.
   [Blaney, D. L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Bell, J. F.; Wellington, D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
   [Clark, B.] Space Sci Inst, Boulder, CO USA.
   [Dyar, M. D.] Mt Holyoke Coll, Dept Earth & Environm & Dept Astron, S Hadley, MA 01075 USA.
   [Ehlmann, B.; Grotzinger, J.; Rice, M.; Stack, K.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA USA.
   [Fabre, C.] Univ Lorraine, CNRS, GeoRessources, UMR7359, Nancy, France.
   [Lewin, E.] Univ Joseph Fourier, ISTerre, Grenoble, France.
   [Leveille, R.] Canadian Space Agcy, St Hubert, PQ, Canada.
   [McLennan, S.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA.
   [Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
   [Sumner, D. Y.] Univ Calif, Earth & Planetary Sci, Davis, CA USA.
   [Vaniman, D.] Planetary Sci Inst, Tucson, AZ USA.
RP Nachon, M (reprint author), Univ Nantes, CNRS, Laboratoire Planetol & Geodynam Nantes, UMR6112, Nantes, France.
EM marion.nachon@univ-nantes.fr
RI Johnson, Jeffrey/F-3972-2015; 
OI Gasnault, Olivier/0000-0002-6979-9012; Clegg, Sam/0000-0002-0338-0948
FU NASA Mars Program Office; Centre National d'Etudes Spatiales (CNES);
   Institut National des Sciences de l'Univers (INSU); Centre National de
   la Recherche Scientifique (CNRS); Observatoire des Sciences de l'Univers
   Nantes Atlantique (OSUNA)
FX We acknowledge P. Sobron and an anonymous reviewer for their revisions.
   Funding in the USA was provided by the NASA Mars Program Office to the
   MSL project. Funding in France was provided by the Centre National
   d'Etudes Spatiales (CNES), the Institut National des Sciences de
   l'Univers (INSU), the Centre National de la Recherche Scientifique
   (CNRS), and the Observatoire des Sciences de l'Univers Nantes Atlantique
   (OSUNA). Data used in this study are available at the Planetary Data
   System (https://pds.jpl.nasa.gov).
NR 79
TC 40
Z9 40
U1 3
U2 48
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 2014
VL 119
IS 9
BP 1991
EP 2016
DI 10.1002/2013JE004588
PG 26
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AR8JH
UT WOS:000343820900001
ER

PT J
AU Moore, JM
   Howard, AD
   Morgan, AM
AF Moore, Jeffrey M.
   Howard, Alan D.
   Morgan, Alexander M.
TI The landscape of Titan as witness to its climate evolution
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Titan climate evolution
ID HUYGENS LANDING SITE; SATURNS MOON TITAN; CASSINI RADAR; SURFACE; LAKES;
   METHANE; TOPOGRAPHY; IMPACTS; MARS; SAR
AB We investigated the range of Titan climate evolution hypotheses regulated by the role, sources, and availability of methane. We analyzed all available image data (principally synthetic aperture radar (SAR)) of Titan's landscape through the T-86 encounter, starting with focused examinations of terrains that carry the markers of climate evolution. Traditional geologic and geomorphic landscape analysis was used to perform morphometric characterization, establish time-stratigraphic relationships, and interpret local and regional geologic process-oriented evolutionary histories. We then assayed the distribution of terrains we identified with respect to both their latitudinal and altimetric occurrence. Our analysis of the terrain types and distributions was used to evaluate and rank the various climate evolution scenarios. We favor progressive hypotheses, which include a relatively brief period in which precipitation was able to affect geomorphic change in low latitudes at scales perceivable in SAR data, with subsequent gradual decline of precipitation intensity coupled with an increasing poleward restriction.
C1 [Moore, Jeffrey M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
   [Howard, Alan D.; Morgan, Alexander M.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA.
RP Moore, JM (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
EM jeff.moore@nasa.gov
RI Morgan, Alexander/J-4850-2012; 
OI Morgan, Alexander/0000-0003-2443-1676; Howard, Alan/0000-0002-5423-1600
FU NASA's Cassini Data Analysis Program
FX We thank Francis Nimmo, Orkan Matt Umurhan, and Don Wilhelms for their
   reviews of the penultimate draft of this paper. We are especially
   grateful for the cogent comments of our journal referees. Thanks goes to
   Carrie Chavez for her help with manuscript preparation and Pam
   Engebretson for her help with figure preparation. NASA's Cassini Data
   Analysis Program supported this research.
NR 100
TC 11
Z9 11
U1 7
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 2014
VL 119
IS 9
BP 2060
EP 2077
DI 10.1002/2014JE004608
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AR8JH
UT WOS:000343820900004
ER

PT J
AU Ruesch, O
   Hiesinger, H
   De Sanctis, MC
   Ammannito, E
   Palomba, E
   Longobardo, A
   Zambon, F
   Tosi, F
   Capria, MT
   Capaccioni, F
   Frigeri, A
   Fonte, S
   Magni, G
   Raymond, CA
   Russell, CT
AF Ruesch, Ottaviano
   Hiesinger, Harald
   De Sanctis, Maria Cristina
   Ammannito, Eleonora
   Palomba, Ernesto
   Longobardo, Andrea
   Zambon, Francesca
   Tosi, Federico
   Capria, Maria Teresa
   Capaccioni, Fabrizio
   Frigeri, Alessandro
   Fonte, Sergio
   Magni, Gianfranco
   Raymond, Carol A.
   Russell, Christopher T.
TI Detections and geologic context of local enrichments in olivine on Vesta
   with VIR/Dawn data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE composition; asteroids; remote sensing; mineralogy; olivine
ID ASTEROID 4 VESTA; PLAGIOCLASE-MAFIC MIXTURES; PARTICLE-SIZE
   DISTRIBUTION; DIOGENITE PARENT BODY; REFLECTANCE SPECTRA; PYROXENE
   MIXTURES; MINERAL MIXTURES; IMPACT BASINS; DARK MATERIAL; MAGMA OCEAN
AB The magmatism characterizing the early history of the asteroid Vesta has long been investigated with the mafic and ultramafic meteorites howardite, eucrite, and diogenite (HED). The lack of geologic context for the meteorites, however, has limited its understanding. Here we use the visible to near-IR (VIR) orbital observations of Vesta's surface to detect relative enrichments in olivine and to study the associated geologic features. Because the near-IR signature of olivine on Vesta's surface is subtle relative to the widespread pyroxene absorption bands, a method was developed to distinguish olivine enrichments from admixture of pyroxenes with high Fe2+/M1, dark material, and potential Fe-bearing glass. Relative enrichment of olivine (similar to<50-60vol %) is found in 2-5km wide, morphologically fresh areas. Our global survey reveals a dozen of these areas clustering in the eastern hemisphere of Vesta. The hemispherical coincidence with a widespread, low enrichment in diogenite-like pyroxene suggests the presence of a distinct compositional terrain. On the central mound of the Rheasilvia impact basin, no olivine enrichment was found, suggesting the absence of an olivine-dominated mantle above the basin's excavation depth or, alternatively, a low amount of olivine homogeneously mixed with diogenite-like pyroxenes. Rare olivine-enriched areas in close proximity to diogenite-like pyroxene are found as part of material ejected by the Rheasilvia impact. Such cooccurrence is reminiscent of local, ultramafic lithologies within the crust. The possible formation of such lithologies on Vesta is supported by some HED meteorites dominated by olivine and orthopyroxene.
C1 [Ruesch, Ottaviano; Hiesinger, Harald] Univ Munster, Inst Planetol, D-48149 Munster, Germany.
   [De Sanctis, Maria Cristina; Ammannito, Eleonora; Palomba, Ernesto; Longobardo, Andrea; Zambon, Francesca; Tosi, Federico; Capria, Maria Teresa; Capaccioni, Fabrizio; Frigeri, Alessandro; Fonte, Sergio; Magni, Gianfranco] INAF, Ist Astrofis Planetol Spaziali, Rome, Italy.
   [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
   [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
RP Ruesch, O (reprint author), Univ Munster, Inst Planetol, D-48149 Munster, Germany.
EM ottaviano.ruesch@uni-muenster.de
RI Frigeri, Alessandro/F-2151-2010; 
OI Frigeri, Alessandro/0000-0002-9140-3977; capria, maria
   teresa/0000-0002-9814-9588; De Sanctis, Maria
   Cristina/0000-0002-3463-4437; Capaccioni, Fabrizio/0000-0003-1631-4314;
   Palomba, Ernesto/0000-0002-9101-6774; Tosi,
   Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592
FU German Aerospace Agency (DLR) [FKZ 50 OW 1102]; NASA Dawn at Vesta
   Participating Scientists Program; Italian Space Agency
FX Discussions with Francois Poulet and the comments of two anonymous
   reviewers helped to improve the manuscript and are acknowledged. Also,
   we acknowledge the financial support of the German Aerospace Agency (DLR
   grant FKZ 50 OW 1102 to O.R.) and the NASA Dawn at Vesta Participating
   Scientists Program. VIR is funded by the Italian Space Agency and was
   developed under the leadership of INAF-Instituto di Astrofisica e
   Planetologia Spaziali, Rome, Italy. The instrument was built by
   Selex-Galileo, Florence, Italy. We thank the German Aerospace Center
   (DLR-PF) and the Max Planck Institute for Solar System Research for the
   development and operation of the Framing Camera as well as for the
   production of FC color filter mosaics. The data used in this study are
   available at the NASA PDS website.
NR 129
TC 17
Z9 17
U1 3
U2 11
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 2014
VL 119
IS 9
BP 2078
EP 2108
DI 10.1002/2014JE004625
PG 31
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AR8JH
UT WOS:000343820900005
ER

PT J
AU Blaney, DL
   Wiens, RC
   Maurice, S
   Clegg, SM
   Anderson, RB
   Kah, LC
   Le Mouelic, S
   Ollila, A
   Bridges, N
   Tokar, R
   Berger, G
   Bridges, JC
   Cousin, A
   Clark, B
   Dyar, MD
   King, PL
   Lanza, N
   Mangold, N
   Meslin, PY
   Newsom, H
   Schroder, S
   Rowland, S
   Johnson, J
   Edgar, L
   Gasnault, O
   Forni, O
   Schmidt, M
   Goetz, W
   Stack, K
   Sumner, D
   Fisk, M
   Madsen, MB
AF Blaney, D. L.
   Wiens, R. C.
   Maurice, S.
   Clegg, S. M.
   Anderson, R. B.
   Kah, L. C.
   Le Mouelic, S.
   Ollila, A.
   Bridges, N.
   Tokar, R.
   Berger, G.
   Bridges, J. C.
   Cousin, A.
   Clark, B.
   Dyar, M. D.
   King, P. L.
   Lanza, N.
   Mangold, N.
   Meslin, P. -Y.
   Newsom, H.
   Schroeder, S.
   Rowland, S.
   Johnson, J.
   Edgar, L.
   Gasnault, O.
   Forni, O.
   Schmidt, M.
   Goetz, W.
   Stack, K.
   Sumner, D.
   Fisk, M.
   Madsen, M. B.
TI Chemistry and texture of the rocks at Rocknest, Gale Crater: Evidence
   for sedimentary origin and diagenetic alteration
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Rocknest; ChemCam; LIBS; Curiosity; Gale
ID INDUCED BREAKDOWN SPECTROSCOPY; CHEMCAM INSTRUMENT SUITE; CURIOSITY
   ROVER; MARS; SCIENCE; CALIBRATION; TRAVERSE; TARGETS; SYSTEM; MAHLI
AB A suite of eight rocks analyzed by the Curiosity Rover while it was stopped at the Rocknest sand ripple shows the greatest chemical divergence of any potentially sedimentary rocks analyzed in the early part of the mission. Relative to average Martian soil and to the stratigraphically lower units encountered as part of the Yellowknife Bay formation, these rocks are significantly depleted in MgO, with a mean of 1.3 wt %, and high in Fe, averaging over 20 wt % FeOT, with values between 15 and 26wt % FeOT. The variable iron and low magnesium and rock texture make it unlikely that these are igneous rocks. Rock surface textures range from rough to smooth, can be pitted or grooved, and show various degrees of wind erosion. Some rocks display poorly defined layering while others seem to show possible fractures. Narrow vertical voids are present in Rocknest 3, one of the rocks showing the strongest layering. Rocks in the vicinity of Rocknest may have undergone some diagenesis similar to other rocks in the Yellowknife Bay Formation as indicated by the presence of soluble calcium phases. The most reasonable scenario is that fine-grained sediments, potentially a mixture of feldspar-rich rocks from Bradbury Rise and normal Martian soil, were lithified together by an iron-rich cement.
C1 [Blaney, D. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
   [Wiens, R. C.; Clegg, S. M.; Cousin, A.; Lanza, N.] Alamos Natl Lab, Los Alamos, NM USA.
   [Maurice, S.; Berger, G.; Meslin, P. -Y.; Schroeder, S.; Gasnault, O.; Forni, O.] Univ Paul Sabatier, Inst Rech Astrophys & Planetol, UPS OMP, Toulouse, France.
   [Anderson, R. B.] S Geol Survey Astrogeol Sci Ctr, Flagstaff, AZ USA.
   [Kah, L. C.] Univ Tennessee, Earth & Planetary Sci, Knoxville, TN USA.
   [Le Mouelic, S.; Mangold, N.] Univ Nantes, CNRS, LPG Nantes, UMR6112, Nantes, France.
   [Ollila, A.; Newsom, H.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
   [Bridges, N.; Johnson, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
   [Tokar, R.] Planetary Sci Inst, Tucson, AZ USA.
   [Bridges, J. C.] Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester, Leics, England.
   [Clark, B.] Space Sci Inst, Boulder, CO USA.
   [Dyar, M. D.] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
   [King, P. L.] Australia Natl Univ, Res Sch Earth Sci, Canberra, ACT, Australia.
   [Rowland, S.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Honolulu, HI USA.
   [Edgar, L.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
   [Schmidt, M.] Brock Univ, Dept Earth Sci, St Catharines, ON, Canada.
   [Goetz, W.] Max Planck Inst Sonnensystemforschung, Katlenburg Lindau, Germany.
   [Stack, K.] CALTECH, Pasadena, CA USA.
   [Sumner, D.] Univ Calif, Dept Geol, Davis, CA USA.
   [Fisk, M.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
   [Madsen, M. B.] Univ Copenhagen, Niels Bohr Inst, Copenhagen, Denmark.
RP Blaney, DL (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM diana.l.blaney@jpl.nasa.gov
RI King, Penelope/A-1791-2011; BERGER, Gilles/F-7118-2016; 
OI King, Penelope/0000-0002-8364-9168; Gasnault,
   Olivier/0000-0002-6979-9012; Clegg, Sam/0000-0002-0338-0948
FU NASA's Mars Exploration Program in the U.S.; CNES in France; Canadian
   Space Agency in Canada; Deutsche Forschungsgemeinschaft (DFG) [GO
   2288/1-1]
FX This work has been conducted at the Jet Propulsion Laboratory,
   California Institute of Technology under a contract with the National
   Aeronautics and Space Administration. This work was funded by NASA's
   Mars Exploration Program in the U.S. and by CNES in France and by the
   Canadian Space Agency in Canada. We acknowledge partial funding by the
   Deutsche Forschungsgemeinschaft (DFG grant GO 2288/1-1) for the
   participation of Walter Goetz. We thank two anonymous reviewers for
   helpful reviews. The many other people who made the MSL mission
   successful are gratefully thanked and acknowledged.
NR 51
TC 17
Z9 17
U1 2
U2 26
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 2014
VL 119
IS 9
BP 2109
EP 2131
DI 10.1002/2013JE004590
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA AR8JH
UT WOS:000343820900006
ER

EF